FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Johnson, MD
Kovalev, YY
Gwinn, CR
Gurvits, LI
Narayan, R
Macquart, JP
Jauncey, DL
Voitsik, PA
Anderson, JM
Sokolovsky, KV
Lisakov, MM
AF Johnson, Michael D.
Kovalev, Yuri Y.
Gwinn, Carl R.
Gurvits, Leonid I.
Narayan, Ramesh
Macquart, Jean-Pierre
Jauncey, David L.
Voitsik, Peter A.
Anderson, James M.
Sokolovsky, Kirill V.
Lisakov, Mikhail M.
TI EXTREME BRIGHTNESS TEMPERATURES AND REFRACTIVE SUBSTRUCTURE IN 3C 273
WITH RADIOASTRON
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: structure; quasars: individual (3C 273); scattering; techniques:
high angular resolution; techniques: interferometric; turbulence
ID SCATTER-BROADENED IMAGE; EXTRAGALACTIC RADIO-SOURCES; INTERFEROMETRIC
VISIBILITIES; INTERSTELLAR SCINTILLATION; VARIABILITY; SIMULATIONS;
SHAPE; SIZE
AB Earth-space interferometry with RadioAstron provides the highest direct angular resolution ever achieved in astronomy at any wavelength. RadioAstron detections of the classic quasar 3C 273 on interferometric baselines up to 171,000 km suggest brightness temperatures exceeding expected limits from the "inverse-Compton catastrophe" by two orders of magnitude. We show that at 18 cm, these estimates most likely arise from refractive substructure introduced by scattering in the interstellar medium. We use the scattering properties to estimate an intrinsic brightness temperature of 7 x 10(12) K, which is consistent with expected theoretical limits, but which is similar to 15 times lower than estimates that neglect substructure. At 6.2 cm, the substructure influences the measured values appreciably but gives an estimated brightness temperature that is comparable to models that do not account for the substructure. At 1.35 cm, the substructure does not affect the extremely high inferred brightness temperatures, in excess of 10(13) K. We also demonstrate that for a source having a Gaussian surface brightness profile, a single long-baseline estimate of refractive substructure determines an absolute minimum brightness temperature, if the scattering properties along a given line of sight are known, and that this minimum accurately approximates the apparent brightness temperature over a wide range of total flux densities.
C1 [Johnson, Michael D.; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kovalev, Yuri Y.; Voitsik, Peter A.; Sokolovsky, Kirill V.; Lisakov, Mikhail M.] Ctr Astro Space, Lebedev Phys Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Kovalev, Yuri Y.; Anderson, James M.] Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany.
[Gwinn, Carl R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Gurvits, Leonid I.] Joint Inst VLBI ERIC, POB 2, NL-7990 AA Dwingeloo, Netherlands.
[Gurvits, Leonid I.] Delft Univ Technol, Dept Astrodynam & Space Missions, NL-2629 HS Delft, Netherlands.
[Macquart, Jean-Pierre] Curtin Univ, Curtin Inst Radio Astron, ICRAR, Perth, WA 6845, Australia.
[Macquart, Jean-Pierre] ARC Ctr Excellence All Sky Astrophys CAASTRO, Melbourne, Vic, Australia.
[Jauncey, David L.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Jauncey, David L.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Anderson, James M.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum GFZ, Dept Geodesy 1, Telegrafenberg, D-14473 Potsdam, Germany.
[Sokolovsky, Kirill V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skii Pr 13, Moscow 119992, Russia.
RP Johnson, MD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mjohnson@cfa.harvard.edu
RI Voytsik, Petr/M-6075-2013; Kovalev, Yuri/J-5671-2013; Lisakov,
Mikhail/M-6034-2013; Sokolovsky, Kirill/D-2246-2015;
OI Kovalev, Yuri/0000-0001-9303-3263; Lisakov, Mikhail/0000-0001-6088-3819;
Sokolovsky, Kirill/0000-0001-5991-6863; Narayan,
Ramesh/0000-0002-1919-2730
FU Gordon and Betty Moore Foundation [GBMF-3561]; Russian Foundation for
Basic Research grant [13-02-12103]
FX M.D.J. thanks the Gordon and Betty Moore Foundation for financial
support of this work through grant GBMF-3561 to Sheperd Doeleman. The
RadioAstron project is led by the Astro Space Center of the Lebedev
Physical Institute of the Russian Academy of Sciences and the Lavochkin
Association of the Russian Federal Space Agency, and is a collaboration
with partner institutions in Russia and other countries. This project
was supported by the Russian Foundation for Basic Research grant
13-02-12103. The Arecibo Observatory is operated by SRI International
under a cooperative agreement with the National Science Foundation
(AST-1100968), and in alliance with Ana G.. Mendez-Universidad
Metropolitana, and the Universities Space Research Association. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. This research is partly based on observations with
the 100 m telescope of the MPIfR (Max-Planck-Institute for Radio
Astronomy) at Effelsberg.
NR 28
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L10
DI 10.3847/2041-8205/820/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000010
ER
PT J
AU Kovalev, YY
Kardashev, NS
Kellermann, KI
Lobanov, AP
Johnson, MD
Gurvits, LI
Voitsik, PA
Zensus, JA
Anderson, JM
Bach, U
Jauncey, DL
Ghigo, F
Ghosh, T
Kraus, A
Kovalev, YA
Lisakov, MM
Petrov, LY
Romney, JD
Salter, CJ
Sokolovsky, KV
AF Kovalev, Y. Y.
Kardashev, N. S.
Kellermann, K. I.
Lobanov, A. P.
Johnson, M. D.
Gurvits, L. I.
Voitsik, P. A.
Zensus, J. A.
Anderson, J. M.
Bach, U.
Jauncey, D. L.
Ghigo, F.
Ghosh, T.
Kraus, A.
Kovalev, Yu. A.
Lisakov, M. M.
Petrov, L. Yu.
Romney, J. D.
Salter, C. J.
Sokolovsky, K. V.
TI RADIOASTRON OBSERVATIONS OF THE QUASAR 3C273: A CHALLENGE TO THE
BRIGHTNESS TEMPERATURE LIMIT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (3C273); radio
continuum: galaxies; techniques: interferometric
ID ACTIVE GALACTIC NUCLEI; COMPACT RADIO-SOURCES; INVERSE COMPTON
CATASTROPHE; BASE-LINE ARRAY; STELLAR SOURCES; 3C 273; JETS; EMISSION;
SUBSTRUCTURE; PARAMETERS
AB Inverse Compton cooling limits the brightness temperature of the radiating plasma to a maximum of 10(11.5) K. Relativistic boosting can increase its observed value, but apparent brightness temperatures much in excess of 1013 K are inaccessible using ground-based very long baseline interferometry (VLBI) at any wavelength. We present observations of the quasar 3C 273, made with the space VLBI mission RadioAstron on baselines up to 171,000. km, which directly reveal the presence of angular structure as small as 26 mu as (2.7 light months) and brightness temperature in excess of 10(13) K. These measurements challenge our understanding of the non-thermal continuum emission in the vicinity of supermassive black holes and require a much higher Doppler factor than what is determined from jet apparent kinematics.
C1 [Kovalev, Y. Y.; Kardashev, N. S.; Voitsik, P. A.; Kovalev, Yu. A.; Lisakov, M. M.; Sokolovsky, K. V.] Ctr Astro Space, Lebedev Phys Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Kovalev, Y. Y.; Lobanov, A. P.; Zensus, J. A.; Anderson, J. M.; Bach, U.; Kraus, A.] Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany.
[Kellermann, K. I.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Lobanov, A. P.] Univ Hamburg, Inst Expt Phys, Luruper Chaussee 147, D-22761 Hamburg, Germany.
[Johnson, M. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Gurvits, L. I.] Joint Inst VLBI ERIC, POB 2, NL-7990 AA Dwingeloo, Netherlands.
[Gurvits, L. I.] Delft Univ Technol, Dept Astrodynam & Space Missions, NL-2629 HS Delft, Netherlands.
[Anderson, J. M.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum, Dept Geodesy & Remote Sensing 1, Telegrafenberg, D-14473 Potsdam, Germany.
[Jauncey, D. L.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Jauncey, D. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Ghigo, F.] Natl Radio Astron Observ, Rt 28-92, Green Bank, WV 24944 USA.
[Ghosh, T.; Salter, C. J.] NAIC, Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA.
[Petrov, L. Yu.] Astrogeo Ctr, 7312 Sportsman Dr, Falls Church, VA 22043 USA.
[Romney, J. D.] Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA.
[Sokolovsky, K. V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skii Prospekt 13, Moscow 119992, Russia.
RP Kovalev, YY (reprint author), Ctr Astro Space, Lebedev Phys Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.; Kovalev, YY (reprint author), Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany.
RI Voytsik, Petr/M-6075-2013; Kovalev, Yuri/J-5671-2013; Lisakov,
Mikhail/M-6034-2013; Kovalev, Yuri/N-1053-2015; Sokolovsky,
Kirill/D-2246-2015; Kardashev, Nikolai/O-6441-2015
OI Kovalev, Yuri/0000-0001-9303-3263; Lisakov, Mikhail/0000-0001-6088-3819;
Sokolovsky, Kirill/0000-0001-5991-6863;
FU Russian Foundation for Basic Research grant [13-02-12103]
FX The RadioAstron project is led by the Astro Space Center of the Lebedev
Physical Institute of the Russian Academy of Sciences and the Lavochkin
Association of the Russian Federal Space Agency, and is a collaboration
with partner institutions in Russia and other countries. The Arecibo
Observatory is operated by SRI International under a cooperative
agreement with the National Science Foundation (AST-1100968), and in
alliance with Ana G. Mendez-Universidad Metropolitana, and the
Universities Space Research Association. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. This
research is partly based on observations with the 100 m telescope of the
MPIfR (Max-Planck-Institute for Radio Astronomy) at Effelsberg. This
research has made use of data from the MOJAVE database, which is
maintained by the MOJAVE team (Lister et al. 2009). We have processed
and used archival VLBA observations at 18 cm (code. BG196I). We would
like to extend thanks to the NRAO group responsible for developing and
deploying phased-array VLBI capabilities at the newly upgraded VLA. We
thank Tuomas Savolainen, Alexander Pushkarev, Richard Schilizzi, Phil
Edwards, Sergio Colafrancesco, and Martin Rees for helpful discussions.
We thank the referee for constructive comments. This project was
supported by the Russian Foundation for Basic Research grant
13-02-12103.
NR 40
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L9
DI 10.3847/2041-8205/820/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000009
ER
PT J
AU Lee, KI
Dunham, MM
Myers, PC
Arce, HG
Bourke, TL
Goodman, AA
Jorgensen, JK
Kristensen, LE
Offner, SSR
Pineda, JE
Tobin, JJ
Vorobyov, EI
AF Lee, Katherine I.
Dunham, Michael M.
Myers, Philip C.
Arce, Hector G.
Bourke, Tyler L.
Goodman, Alyssa A.
Jorgensen, Jes K.
Kristensen, Lars E.
Offner, Stella S. R.
Pineda, Jaime E.
Tobin, John J.
Vorobyov, Eduard I.
TI MISALIGNMENT OF OUTFLOW AXES IN THE PROTO-MULTIPLE SYSTEMS IN PERSEUS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; ISM: kinematics and dynamics; ISM: molecules; stars:
formation; stars: protostars; submillimeter: ISM
ID HYDROSTATIC CORE CANDIDATES; YOUNGEST PROTOSTARS; STAR-FORMATION;
MOLECULAR JET; BINARY-SYSTEM; BROWN DWARF; STELLAR; DISKS; NGC-1333;
FRAGMENTATION
AB We investigate the alignment between outflow axes in nine of the youngest binary/multiple systems in the Perseus Molecular Cloud. These systems have typical member spacing larger than 1000 au. For outflow identification, we use (CO)-C-12(2-1) and (CO)-C-12(3-2) data from a large survey with the Submillimeter Array: Mass Assembly of Stellar Systems and their Evolution with the SMA. The distribution of outflow orientations in the binary pairs is consistent with random or preferentially anti-aligned distributions, demonstrating that these outflows are misaligned. This result suggests that these systems are possibly formed in environments where the distribution of angular momentum is complex and disordered, and these systems do not come from the same co-rotating structures or from an initial cloud with aligned vectors of angular momentum.
C1 [Lee, Katherine I.; Dunham, Michael M.; Myers, Philip C.; Bourke, Tyler L.; Goodman, Alyssa A.; Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Bourke, Tyler L.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England.
[Jorgensen, Jes K.] Univ Copenhagen, Niels Bohr Inst & Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Offner, Stella S. R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Pineda, Jaime E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Tobin, John J.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Vorobyov, Eduard I.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria.
[Vorobyov, Eduard I.] Southern Fed Univ, Inst Phys Res, Rostov Na Donu 344090, Russia.
RP Lee, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM katherine.lee@cfa.harvard.edu
RI Kristensen, Lars/F-4774-2011;
OI Kristensen, Lars/0000-0003-1159-3721; Goodman,
Alyssa/0000-0003-1312-0477
FU Smithsonian Institution; Academia Sinica; NASA [NNX14AG96G]; NASA ADAP
grant [NNX13AE54G]; Submillimeter Array through an SMA postdoctoral
fellowship; National Aeronautics and Space Administration
[14-ATP14-0078]; Netherlands Organisation for Scientific Research (NWO)
[639.041.439]; Russian Ministry of Education and Science [3.961.2014/K]
FX This work is based primarily on observations obtained with the SMA, a
joint project between the Smithsonian Astrophysical Observatory and the
Academia Sinica Institute of Astronomy and Astrophysics and funded by
the Smithsonian Institution and the Academia Sinica. The authors thank
the SMA staff for executing these observations as part of the queue
schedule, and Charlie Qi and Mark Gurwell for their technical assistance
with the SMA data.; K.I.L. acknowledges support from NASA grant
NNX14AG96G. M.M.D. acknowledges support from NASA ADAP grant NNX13AE54G
and from the Submillimeter Array through an SMA postdoctoral fellowship.
T.L.B. also acknowledges partial support from NASA ADAP grant
NNX13AE54G. E.I.V. acknowledges support from the Russian Ministry of
Education and Science grant 3.961.2014/K. SSRO acknowledges support from
the National Aeronautics and Space Administration under grant No.
14-ATP14-0078 issued through the Astrophysics Theory Program. J.J.T. is
currently supported by grant 639.041.439 from the Netherlands
Organisation for Scientific Research (NWO).
NR 46
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L2
DI 10.3847/2041-8205/820/1/L2
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000002
ER
PT J
AU Yamaguchi, H
Katsuda, S
Castro, D
Williams, BJ
Lopez, LA
Slane, PO
Smith, RK
Petre, R
AF Yamaguchi, Hiroya
Katsuda, Satoru
Castro, Daniel
Williams, Brian J.
Lopez, Laura A.
Slane, Patrick O.
Smith, Randall K.
Petre, Robert
TI THE REFINED SHOCK VELOCITY OF THE X-RAY FILAMENTS IN THE RCW 86
NORTHEAST RIM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; ISM: individual objects (RCW 86); ISM:
supernova remnants; proper motions; shock waves; X-rays: ISM
ID SUPERNOVA REMNANT RCW-86; FE-RICH EJECTA; PROPER MOTIONS;
BALMER-FILAMENTS; IA SUPERNOVA; SN 1006; EMISSION; SHELL; EFFICIENCY;
DISCOVERY
AB A precise measurement of shock velocities is crucial for constraining the mechanism and efficiency of cosmic-ray (CR) acceleration at supernova remnant (SNR) shock fronts. The northeastern rim of the SNR RCW 86 is thought to be a particularly efficient CR acceleration site, owing to the recent result in which an extremely high shock velocity of similar to 6000 km s(-1) was claimed. Here, we revisit the same SNR rim with the Chandra X-ray Observatory, 11 years after the first observation. This longer baseline than previously available allows us to determine a more accurate proper motion of the nonthermal X-ray filament, revealing a much lower velocity of 3000 +/- 340 km s(-1) (and even slower at a brighter region). Although the value has dropped to one-half of that from the previous X-ray measurement, it is still higher than the mean velocity of the H alpha filaments in this region (similar to 1200 km s(-1)). This discrepancy implies that the filaments bright in nonthermal X-rays and H alpha emission trace different velocity components, and thus a CR pressure constrained by combining the X-ray kinematics and the H alpha spectroscopy can easily be overestimated. We also measure the proper motion of the thermal X-ray filament immediately to the south of the nonthermal one. The inferred velocity (720 +/- 360 km s(-1)) is significantly lower than that of the nonthermal filament, suggesting the presence of denser ambient material, possibly a wall formed by a wind from the progenitor, which has drastically slowed down the shock.
C1 [Yamaguchi, Hiroya; Castro, Daniel; Williams, Brian J.; Petre, Robert] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Katsuda, Satoru] JAXA, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
[Lopez, Laura A.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Lopez, Laura A.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.; Yamaguchi, H (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM hiroya.yamaguchi@nasa.gov
OI Williams, Brian/0000-0003-2063-381X
FU Chandra GO Program [GO5-16072A]
FX We thank Dr. Ryo Yamazaki for helpful discussion at Harvard-Smithsonian
Center for Astrophysics. This work is supported by the Chandra GO
Program grant GO5-16072A.
NR 29
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L3
DI 10.3847/2041-8205/820/1/L3
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000003
ER
PT J
AU Davies, N
Field, D
Gavaghan, D
Holbrook, SJ
Planes, S
Troyer, M
Bonsall, M
Claudet, J
Roderick, G
Schmitt, RJ
Zettler, LA
Berteaux, V
Bossin, HC
Cabasse, C
Collin, A
Deck, J
Dell, T
Dunne, J
Gates, R
Harfoot, M
Hench, JL
Hopuare, M
Kirch, P
Kotoulas, G
Kosenkov, A
Kusenko, A
Leichter, JJ
Lenihan, H
Magoulas, A
Martinez, N
Meyer, C
Stoll, B
Swalla, B
Tartakovsky, DM
Murphy, HT
Turyshev, S
Valdvinos, F
Williams, R
Wood, S
AF Davies, Neil
Field, Dawn
Gavaghan, David
Holbrook, Sally J.
Planes, Serge
Troyer, Matthias
Bonsall, Michael
Claudet, Joachim
Roderick, George
Schmitt, Russell J.
Zettler, Linda Amaral
Berteaux, Veronique
Bossin, Herve C.
Cabasse, Charlotte
Collin, Antoine
Deck, John
Dell, Tony
Dunne, Jennifer
Gates, Ruth
Harfoot, Mike
Hench, James L.
Hopuare, Marania
Kirch, Patrick
Kotoulas, Georgios
Kosenkov, Alex
Kusenko, Alex
Leichter, James J.
Lenihan, Hunter
Magoulas, Antonios
Martinez, Neo
Meyer, Chris
Stoll, Benoit
Swalla, Billie
Tartakovsky, Daniel M.
Murphy, Hinano Teavai
Turyshev, Slava
Valdvinos, Fernanda
Williams, Rich
Wood, Spencer
CA IDEA Consortium
TI Simulating social-ecological systems: the Island Digital Ecosystem
Avatars (IDEA) consortium
SO GIGASCIENCE
LA English
DT Editorial Material
DE Computational ecology; Biodiversity; Genomics; Biocode; Earth
observations; Social-ecological system; Ecosystem dynamics; Climate
change scenarios; Predictive modeling
ID INTERGOVERNMENTAL PLATFORM; MODEL; SCIENCE; BIODIVERSITY
AB Systems biology promises to revolutionize medicine, yet human wellbeing is also inherently linked to healthy societies and environments (sustainability). The IDEA Consortium is a systems ecology open science initiative to conduct the basic scientific research needed to build use-oriented simulations (avatars) of entire social-ecological systems. Islands are the most scientifically tractable places for these studies and we begin with one of the best known: Moorea, French Polynesia. The Moorea IDEA will be a sustainability simulator modeling links and feedbacks between climate, environment, biodiversity, and human activities across a coupled marine-terrestrial landscape. As a model system, the resulting knowledge and tools will improve our ability to predict human and natural change on Moorea and elsewhere at scales relevant to management/conservation actions.
C1 [Davies, Neil] Univ Calif Berkeley, Gump South Pacific Res Stn, BP 244, Moorea 98728, Fr Polynesia.
[Davies, Neil; Field, Dawn; Bonsall, Michael] Univ Oxford, Dept Zool, Biodivers Inst, Tinbergen Bldg,South Parks Rd, Oxford OX1 3PS, England.
[Davies, Neil; Cabasse, Charlotte] Univ Calif Berkeley, Berkeley Inst Data Sci, 190 Doe Lib, Berkeley, CA 94720 USA.
[Gavaghan, David] Univ Oxford, Dept Comp Sci, Computat Biol Grp, Wolfson Bldg, Oxford, England.
[Holbrook, Sally J.; Schmitt, Russell J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Holbrook, Sally J.; Schmitt, Russell J.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
[Planes, Serge; Claudet, Joachim; Berteaux, Veronique] CRIOBE, Lab Excellence CORAIL, USR CNRS EPHE UPVD 3278, BP 1013, Papetoai 98729, Moorea, Fr Polynesia.
[Troyer, Matthias; Kosenkov, Alex] Swiss Fed Inst Technol, Inst Theoret Phys & Platform Adv Sci Comput, CH-8093 Zurich, Switzerland.
[Roderick, George] Univ Calif Berkeley, Dept Environm Sci Policy & Management, 130 Mulford Hall 3114, Berkeley, CA 94720 USA.
[Zettler, Linda Amaral] Inst Marine Biol, Josephine Bay Paul Ctr Comparat Mol Biol & Evolut, Woods Hole, MA 02543 USA.
[Bossin, Herve C.] Inst Louis Malarde, Unit Med Entomol, BP 30, Tahiti 98713, Fr Polynesia.
[Collin, Antoine] Ecole Prat Hautes Etud, Lab Coastal Geomorphol & Environm, Dinard, France.
[Deck, John] Berkeley Nat Hist Museums, 3101 Valley Life Sci Bldg, Berkeley, CA 94720 USA.
[Dell, Tony] NGRREC, 1 Confluence Way, East Alton, IL 62024 USA.
[Dunne, Jennifer] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Gates, Ruth] Univ Hawaii Manoa, Hawaii Inst Marine Biol, Sch Ocean & Earth Sci & Technol, POB 1346, Kaneohe, HI 96744 USA.
[Harfoot, Mike] United Nations Environm Programme World Conservat, 219 Huntingdon Rd, Cambridge CB3 0DL, England.
[Hench, James L.] Duke Univ, Nicholas Sch Environm, Marine Lab, 135 Marine Lab Rd, Beaufort, NC 28516 USA.
[Hopuare, Marania; Stoll, Benoit] Univ Polynesie Francaise, Lab GePaSud, Tahiti BP6570, Faaa, Fr Polynesia.
[Kirch, Patrick] Univ Calif Berkeley, Dept Anthropol, 232 Kroeber Hall, Berkeley, CA 94720 USA.
[Kotoulas, Georgios; Magoulas, Antonios] Biotechnol & Aquaculture Hellen Ctr Marine Res Go, Inst Marine Biol, POB 2214, GR-71003 Iraklion, Crete, Greece.
[Kusenko, Alex] Univ Calif Los Angeles, Dept Phys & Astron, 475 Portola Plaza, Los Angeles, CA 90095 USA.
[Leichter, James J.] Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Lenihan, Hunter] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, 3428 Bren Hall, Santa Barbara, CA 93106 USA.
[Martinez, Neo; Valdvinos, Fernanda] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
[Martinez, Neo] Pacific Ecoinformat & Computat Ecol Lab, Berkeley, CA 94703 USA.
[Meyer, Chris] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA.
[Swalla, Billie] Univ Washington, Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA.
[Tartakovsky, Daniel M.] Univ Calif San Diego, Dept Mech & Aerosp Engn, 9500 Gilman Dr,Mail Code 0411, La Jolla, CA 92093 USA.
[Murphy, Hinano Teavai] Univ Calif Berkeley, Gump Stn, Atitia Ctr, BP 244, Moorea 98728, Fr Polynesia.
[Turyshev, Slava] CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Turyshev, Slava] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Turyshev, Slava] Univ Calif Los Angeles, Dept Earth & Planetary Sci, Los Angeles, CA 90095 USA.
[Williams, Rich] Vibrant Data Inc, 943 Clay St, San Francisco, CA 94108 USA.
[Wood, Spencer] Univ Washington, Sch Environm & Forest Sci, Box 352100, Seattle, WA 98195 USA.
[IDEA Consortium] Swiss Fed Inst Technol, IDEA Consortium, Zurich, Switzerland.
RP Davies, N (reprint author), Univ Calif Berkeley, Gump South Pacific Res Stn, BP 244, Moorea 98728, Fr Polynesia.; Troyer, M (reprint author), Swiss Fed Inst Technol, Inst Theoret Phys & Platform Adv Sci Comput, CH-8093 Zurich, Switzerland.
EM ndavies@moorea.berkeley.edu; troyer@phys.ethz.ch
RI Claudet, Joachim/C-6335-2008; Martinez, Neo/A-5312-2008; Troyer,
Matthias/B-7826-2008; Davies, Neil/E-5863-2012;
OI Claudet, Joachim/0000-0001-6295-1061; Martinez, Neo/0000-0002-1130-5550;
Troyer, Matthias/0000-0002-1469-9444; Davies, Neil/0000-0001-8085-5014;
Collin, Antoine/0000-0001-9559-7572; BOSSIN, Herve/0000-0002-3655-0923;
gavaghan, david/0000-0001-8311-3200
NR 19
TC 1
Z9 1
U1 4
U2 30
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
EI 2047-217X
J9 GIGASCIENCE
JI GigaScience
PD MAR 17
PY 2016
VL 5
AR 14
DI 10.1186/s13742-016-0118-5
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9UA
UT WOS:000372428100001
PM 26998258
ER
PT J
AU Freeman, CJ
Easson, CG
AF Freeman, Christopher J.
Easson, Cole G.
TI Sponge distribution and the presence of photosymbionts in Moorea, French
Polynesia
SO PEERJ
LA English
DT Article
DE Symbiosis; Photosymbionts; Porifera; Biodiversity; Moorea; Mutualism
ID CYANOBACTERIUM OSCILLATORIA-SPONGELIAE; 4 DICTYOCERATID SPONGES;
CORAL-REEF SPONGES; SPATIAL-PATTERNS; MARINE SPONGES; PRODUCTIVITY;
SYMBIOSES; ABUNDANCE; DIVERSITY; EVOLUTION
AB Photosymbionts play an important role in the ecology and evolution of diverse host species within the marine environment Although sponge-photosymbiont interactions have been well described from geographically disparate sites worldwide, our understanding of these interactions from shallow water systems within French Polynesia is limited. We surveyed diverse habitats around the north coast of Moorea, French Polynesia and screened sponges for the presence of photosymbionts. Overall sponge abundance and diversity were low, with <1% cover and only eight putative species identified by 28S barcoding from surveys at 21 sites. Of these eight species, seven were found predominately in shaded or semi-cryptic habitats under overhangs or within caverns. Lendenfeldia chondrodes was the only species that supported a high abundance of photosymbionts and was also the only species found in exposed, illuminated habitats. Interestingly, L. chondrodes was found at three distinct sites, with a massive, fan-shaped growth form at two of the lagoon sites and a thin, encrusting growth form within a bay site. These two growth forrns differed in their photosymbiont abundance, with massive individuals of L. chondrodes having higher photosymbiont abundance than encrusting individuals from the bay. We present evidence that some sponges from French Polynesia support abundant photosymbiont communities and provide initial support for the role of these communities in host ecology.
C1 [Freeman, Christopher J.] Smithsonian Marine Stn, Ft Pierce, FL USA.
[Freeman, Christopher J.] IRCP, Papetoai, Moorea, Fr Polynesia.
[Easson, Cole G.] Nova SE Univ, Halmos Coll Nat Sci & Oceanog, Dania, FL USA.
[Easson, Cole G.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA.
RP Freeman, CJ (reprint author), Smithsonian Marine Stn, Ft Pierce, FL USA.; Freeman, CJ (reprint author), IRCP, Papetoai, Moorea, Fr Polynesia.
EM freemanc@si.edu
FU Institute for Pacific Coral Reefs (IRCP); Smithsonian MarineGEO and
Tennenbaum Marine Observatories Network
FX This work was supported by a research grant awarded to CJF from the
Institute for Pacific Coral Reefs (IRCP), as well as a postdoctoral
fellowship awarded to CJF from the Smithsonian MarineGEO and Tennenbaum
Marine Observatories Network. The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 42
TC 2
Z9 2
U1 7
U2 14
PU PEERJ INC
PI LONDON
PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND
SN 2167-8359
J9 PEERJ
JI PeerJ
PD MAR 17
PY 2016
VL 4
AR e1816
DI 10.7717/peerj.1816
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH1XQ
UT WOS:000372578700004
PM 27014516
ER
PT J
AU Hung, CM
Drovetski, SV
Zink, RM
AF Hung, Chih-Ming
Drovetski, Sergei V.
Zink, Robert M.
TI Matching loci surveyed to questions asked in phylogeography
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE mitochondrial DNA; nuclear genes; Z-linked; phylogeography; coalescence
ID MOLECULAR EVOLUTION; MITOCHONDRIAL-DNA; POPULATION-SIZE; NUCLEOTIDE
DIVERSITY; NUCLEAR INTRONS; AVIAN GENOME; Z-CHROMOSOME; DIVERGENCE;
SELECTION; SEQUENCES
AB Although mitochondrial DNA (mtDNA) has long been used for assessing genetic variation within and between populations, its workhorse role in phylogeography has been criticized owing to its single-locus nature. The only choice for testing mtDNA results is to survey nuclear loci, which brings into contrast the difference in locus effective size and coalescence times. Thus, it remains unclear how erroneous mtDNA-based estimates of species history might be, especially for evolutionary events in the recent past. To test the robustness of mtDNA and nuclear sequences in phylogeography, we provide one of the largest paired comparisons of summary statistics and demographic parameters estimated from mitochondrial, five Z-linked and 10 autosomal genes of 30 avian species co-distributed in the Caucasus and Europe. The results suggest that mtDNA is robust in estimating inter-population divergence but not in intra-population diversity, which is sensitive to population size change. Here, we provide empirical evidence showing that mtDNA was more likely to detect population divergence than any other single locus owing to its smaller N-e and thus faster coalescent time. Therefore, at least in birds, numerous studies that have based their inferences of phylogeographic patterns solely on mtDNA should not be readily dismissed.
C1 [Hung, Chih-Ming] Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan.
[Drovetski, Sergei V.] Smithsonian Inst, Div Birds, Natl Museum Nat Hist, Washington, DC 20004 USA.
[Zink, Robert M.] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA.
[Zink, Robert M.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
RP Hung, CM (reprint author), Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan.
EM ymwur1@gmail.com
RI Drovetski, Sergei/A-6002-2011
OI Drovetski, Sergei/0000-0002-1832-5597
FU NSF [DEB 0919494]; Fundos FEDER funds through the COMPETE program;
Fundacao pars a Ciencia e a Tecnologia, Portugal
[FCOMP-01-0124-FEDER-008941, PTDC/BIA-BEC/103435/2008]
FX Support came from NSF (DEB 0919494) to R.M.Z. and from Fundos FEDER
funds through the COMPETE program and the Fundacao pars a Ciencia e a
Tecnologia, Portugal (FCOMP-01-0124-FEDER-008941; FCT reference
PTDC/BIA-BEC/103435/2008) to S.V.D.
NR 60
TC 0
Z9 0
U1 4
U2 5
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD MAR 16
PY 2016
VL 283
IS 1826
AR 20152340
DI 10.1098/rspb.2015.2340
PG 8
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DK4WV
UT WOS:000374921900019
PM 26962145
ER
PT J
AU van der Zee, EM
Angelini, C
Govers, LL
Christianen, MJA
Altieri, AH
van der Reijden, KJ
Silliman, BR
De Koppel, JV
van der Geest, M
van Gils, JA
van der Veer, HW
Piersma, T
de Ruiter, PC
Olff, H
van der Heide, T
AF van der Zee, Els M.
Angelini, Christine
Govers, Laura L.
Christianen, Marjolijn J. A.
Altieri, Andrew H.
van der Reijden, Karin J.
Silliman, Brian R.
De Koppel, Johan van
van der Geest, Matthijs
van Gils, Jan A.
van der Veer, Henk W.
Piersma, Theunis
de Ruiter, Peter C.
Olff, Han
van der Heide, Tjisse
TI How habitat-modifying organisms structure the food web of two coastal
ecosystems
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE consumer-resource interactions; non-trophic interactions; facilitation;
ecological networks; ecosystem engineering; foundation species
ID COMMUNITY STRUCTURE; NETWORK STRUCTURE; FACILITATION; STABILITY; MODEL;
CONNECTANCE; INCREASES; REAL
AB The diversity and structure of ecosystems has been found to depend both on trophic interactions in food webs and on other species interactions such as habitat modification and mutualism that form non-trophic interaction networks. However, quantification of the dependencies between these two main interaction networks has remained elusive. In this study, we assessed how habitat-modifying organisms affect basic food web properties by conducting in-depth empirical investigations of two ecosystems: North American temperate fringing marshes and West African tropical seagrass meadows. Results reveal that habitat-modifying species, through non-trophic facilitation rather than their trophic role, enhance species richness across multiple trophic levels, increase the number of interactions per species (link density), but decrease the realized fraction of all possible links within the food web (connectance). Compared to the trophic role of the most highly connected species, we found this non-trophic effects to be more important for species richness and of more or similar importance for link density and connectance. Our findings demonstrate that food webs can be fundamentally shaped by interactions outside the trophic network, yet intrinsic to the species participating in it. Better integration of non-trophic interactions in food web analyses may therefore strongly contribute to their explanatory and predictive capacity.
C1 [van der Zee, Els M.; Christianen, Marjolijn J. A.; van der Reijden, Karin J.; De Koppel, Johan van; Piersma, Theunis; Olff, Han; van der Heide, Tjisse] Univ Groningen, Groningen Inst Evolutionary Life Sci, POB 11103, NL-9700 CC Groningen, Netherlands.
[van der Zee, Els M.; van der Geest, Matthijs; van Gils, Jan A.; van der Veer, Henk W.; Piersma, Theunis] NIOZ Royal Netherlands Inst Sea Res, Dept Marine Ecol, POB 59, NL-1790 AB Den Burg, Texel, Netherlands.
[van der Zee, Els M.] Altenburg & Wymenga Ecol Consultants, Suderwei 2, NL-9269 TZ Veenwouden, Netherlands.
[Angelini, Christine] Univ Florida, Dept Environm Engn Sci, Gainesville, FL 32611 USA.
[Govers, Laura L.; van der Heide, Tjisse] Radboud Univ Nijmegen, Inst Wetland & Water Res, Aquat Ecol & Environm Biol Grp, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
[Altieri, Andrew H.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[van der Reijden, Karin J.] Inst Marine Resources & Ecosyst, Haringkade 1, NL-1976 CP Ijmuiden, Netherlands.
[Silliman, Brian R.] Duke Univ, Div Marine Sci & Conservat, Beaufort, NC 28516 USA.
[De Koppel, Johan van] NIOZ Royal Netherlands Inst Sea Res, Ctr Estuarine & Marine Ecol, POB 140, NL-4400 AC Yerseke, Netherlands.
[de Ruiter, Peter C.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, POB 94248, NL-1090 GE Amsterdam, Netherlands.
RP Olff, H (reprint author), Univ Groningen, Groningen Inst Evolutionary Life Sci, POB 11103, NL-9700 CC Groningen, Netherlands.
EM h.olff@rug.nl
RI Olff, Han/A-8516-2008; van Gils, Jan/B-5544-2008; van der Heide,
Tjisse/M-3000-2013; van der Geest, Matthijs/A-4744-2013; Christianen,
Marjolijn/B-8847-2011; van der Veer, Henk/I-5383-2016
OI Olff, Han/0000-0003-2154-3576; van Gils, Jan/0000-0002-4132-8243; van
der Geest, Matthijs/0000-0002-9837-3803; Christianen,
Marjolijn/0000-0001-5839-2981; van der Veer, Henk/0000-0001-5035-661X
FU 'Waddenfonds' programme; NSF GRFP award [DGE-0802270]; University of
Florida Graduate Alumni Fellowship award; NSF Career award [1056980];
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)-WOTRO
Integrated Programme grant [W.01.65.221.00]; NWO-VIDI grant
[864.09.002]; NWO-VENI grant [863.12.003]
FX E.v.d.Z. and H.O. were financially supported by the 'Waddenfonds'
programme; C.A. by NSF GRFP DGE-0802270 and University of Florida
Graduate Alumni Fellowship awards; B.R.S. by NSF Career award 1056980;
M.v.d.G. and T.P. by the Nederlandse Organisatie voor Wetenschappelijk
Onderzoek (NWO)-WOTRO Integrated Programme grant W.01.65.221.00 awarded
to T.P.; J.v.G. by NWO-VIDI grant 864.09.002; T.v.d.H. by NWO-VENI grant
863.12.003.
NR 47
TC 3
Z9 3
U1 22
U2 54
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD MAR 16
PY 2016
VL 283
IS 1826
AR 20152326
DI 10.1098/rspb.2015.2326
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DK4WV
UT WOS:000374921900022
PM 26962135
ER
PT J
AU Herlihy, MV
Talamas, EJ
Weber, DC
AF Herlihy, Megan V.
Talamas, Elijah J.
Weber, Donald C.
TI Attack and Success of Native and Exotic Parasitoids on Eggs of
Halyomorpha halys in Three Maryland Habitats
SO PLOS ONE
LA English
DT Article
ID PODISUS-MACULIVENTRIS HEMIPTERA; MARMORATED STINK BUG; ASHMEAD
HYMENOPTERA; NATURAL ENEMIES; NORTH-AMERICA; PENTATOMIDAE; HETEROPTERA;
SCELIONIDAE; ATTRACTION; MORTALITY
AB Egg parasitoids of the exotic invasive brown marmorated stink bug, Halyomorpha halys (Stal), were investigated using lab-reared fresh (live) and frozen (killed) lab-reared sentinel egg masses deployed for 72h on foliage in three habitats-woods, orchard, and soybean field-in Maryland, USA, in summer 2014. Four native hymenopteran species, Telenomus podisi Ashmead (Scelionidae), Trissolcus euschisti (Ashmead) and Tr. brochymenae Ashmead (Scelionidae), and Anastatus reduvii (Howard) (Eupelmidae), developed and emerged from H. halys eggs. One exotic parasitoid, Trissolcus japonicus (Ashmead), emerged, providing the first known occurrence of this species in North America. Native parasitoids emerged from frozen eggs significantly more often than from fresh eggs (89.3% of egg masses and 98.1% of individual eggs), whereas the exotic Tr. japonicus did not show a similar difference, strongly suggesting adaptation to H. halys as a host by Tr. japonicus but not by the native species. Parasitoids were habitat-specific: all three Trissolcus species were significantly more likely to occur in the woods habitat, whereas Te. podisi was found exclusively in the soybean field. Further investigations are required to elucidate evolving host-parasitoid relationships, habitat specificity, and non-target effects of Tr. japonicus over the expanded range of H. halys in North America.
C1 [Herlihy, Megan V.; Weber, Donald C.] ARS, Invas Insect Biocontrol & Behav Lab, USDA, Beltsville, MD USA.
[Talamas, Elijah J.] ARS, Systemat Entomol Lab, USDA, Washington, DC USA.
[Talamas, Elijah J.] Smithsonian Inst, Washington, DC 20560 USA.
RP Weber, DC (reprint author), ARS, Invas Insect Biocontrol & Behav Lab, USDA, Beltsville, MD USA.
EM Don.Weber@ars.usda.gov
FU Systematic Entomology Laboratory; Invasive Insect Biocontrol and
Behavior Laboratory, USDA ARS
FX This work was made possible by funding from the Systematic Entomology
Laboratory and the Invasive Insect Biocontrol and Behavior Laboratory,
USDA ARS. Mention of trade names or commercial products in this
publication is solely for the purpose of providing specific information
and does not imply recommendation or endorsement by the USDA; USDA is an
equal opportunity provider and employer.
NR 25
TC 6
Z9 6
U1 14
U2 31
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 16
PY 2016
VL 11
IS 3
AR e0150275
DI 10.1371/journal.pone.0150275
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH1WF
UT WOS:000372574900030
PM 26983012
ER
PT J
AU Lafferriere, NAR
Antelo, R
Alda, F
Martensson, D
Hailer, F
Castroviejo-Fisher, S
Ayarzaguena, J
Ginsberg, JR
Castroviejo, J
Doadrio, I
Vila, C
Amato, G
AF Lafferriere, Natalia A. Rossi
Antelo, Rafael
Alda, Fernando
Martensson, Dick
Hailer, Frank
Castroviejo-Fisher, Santiago
Ayarzagueena, Jose
Ginsberg, Joshua R.
Castroviejo, Javier
Doadrio, Ignacio
Vila, Carles
Amato, George
TI Multiple Paternity in a Reintroduced Population of the Orinoco Crocodile
(Crocodylus intermedius) at the El Frio Biological Station, Venezuela
SO PLOS ONE
LA English
DT Article
ID GENETIC DIVERSITY; SPERM STORAGE; AMERICAN ALLIGATOR; PARENTAGE
ANALYSIS; MATING SYSTEMS; MATE CHOICE; REPRODUCTIVE SUCCESS;
NATURAL-POPULATIONS; MICROSATELLITE DATA; GENOTYPING ERRORS
AB The success of a reintroduction program is determined by the ability of individuals to reproduce and thrive. Hence, an understanding of the mating system and breeding strategies of reintroduced species can be critical to the success, evaluation and effective management of reintroduction programs. As one of the most threatened crocodile species in the world, the Orinoco crocodile (Crocodylus intermedius) has been reduced to only a few wild populations in the Llanos of Venezuela and Colombia. One of these populations was founded by reintroduction at Cano Macanillal and La Ramera lagoon within the El Frio Biological Station, Venezuela. Twenty egg clutches of C. intermedius were collected at the El Frio Biological Station for incubation in the lab and release of juveniles after one year. Analyzing 17 polymorphic microsatellite loci from 335 hatchlings we found multiple paternity in C. intermedius, with half of the 20 clutches fathered by two or three males. Sixteen mothers and 14 fathers were inferred by reconstruction of multilocus parental genotypes. Our findings showed skewed paternal contributions to multiple-sired clutches in four of the clutches (40%), leading to an overall unequal contribution of offspring among fathers with six of the 14 inferred males fathering 90% of the total offspring, and three of those six males fathering more than 70% of the total offspring. Our results provide the first evidence of multiple paternity occurring in the Orinoco crocodile and confirm the success of reintroduction efforts of this critically endangered species in the El Frio Biological Station, Venezuela.
C1 [Lafferriere, Natalia A. Rossi; Ginsberg, Joshua R.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA.
[Lafferriere, Natalia A. Rossi; Amato, George] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA.
[Antelo, Rafael] Fdn Palmarito Casanare, Bogota, Colombia.
[Antelo, Rafael; Alda, Fernando; Doadrio, Ignacio] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolutiva, E-28006 Madrid, Spain.
[Antelo, Rafael; Ayarzagueena, Jose; Castroviejo, Javier] Estn Biol Frio, Apure, Venezuela.
[Alda, Fernando] Louisiana State Univ, Dept Biol Sci, LSU Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Martensson, Dick] Uppsala Univ, Dept Evolutionary Biol, Uppsala, Sweden.
[Hailer, Frank] Cardiff Univ, Sch Biosci, Cardiff CF10 3AX, S Glam, Wales.
[Hailer, Frank] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Castroviejo-Fisher, Santiago] Pontificia Univ Catolica Rio Grande Sul PUCRS, Lab Sistemat Vertebrados, Porto Alegre, RS, Brazil.
[Ginsberg, Joshua R.] Cary Inst Ecosyst Studies, Millbrook, NY USA.
[Castroviejo, Javier] Asociac Amigos Donana, Seville, Spain.
[Vila, Carles] CSIC, EBD, Conservat & Evolutionary Genet Grp, E-41080 Seville, Spain.
RP Lafferriere, NAR (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA.; Lafferriere, NAR (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA.
EM nar2118@columbia.edu
RI CSIC, EBD Donana/C-4157-2011; Castroviejo-Fisher, Santiago/G-9007-2013
OI CSIC, EBD Donana/0000-0003-4318-6602; Castroviejo-Fisher,
Santiago/0000-0002-1048-2168
FU Department of Evolutionary biology, Uppsala University, Uppsala, Sweden;
Dpto. Biodiversidad y Biologia Evolutiva, Museo Nacional de Ciencias
Naturales, CSIC, Madrid, Spain; Sackler Institute of Comparative
Genomics at the American Museum of Natural History (NARL)
FX Funders included the Department of Evolutionary biology, Uppsala
University, Uppsala, Sweden (DM), to support fieldwork and laboratory
work; Dpto. Biodiversidad y Biologia Evolutiva, Museo Nacional de
Ciencias Naturales, CSIC, Madrid, Spain (RA FA SCF ID), to support
fieldwork and laboratory work; Sackler Institute of Comparative Genomics
at the American Museum of Natural History (NARL), to support data
analysis and preparation of manuscript.
NR 95
TC 2
Z9 2
U1 14
U2 22
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 16
PY 2016
VL 11
IS 3
AR e0150245
DI 10.1371/journal.pone.0150245
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH1WF
UT WOS:000372574900027
ER
PT J
AU Ilton, ES
Post, JE
Heaney, PJ
Ling, FT
Kerisit, SN
AF Ilton, Eugene S.
Post, Jeffrey E.
Heaney, Peter J.
Ling, Florence T.
Kerisit, Sebastien N.
TI XPS determination of Mn oxidation states in Mn (hydr)oxides
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE XPS; Manganese; Valence; Birnessite; Catalysis; Oxidation
ID X-RAY-DIFFRACTION; MANGANESE OXIDE MINERALS; NA-RICH BIRNESSITE;
CHROMIUM(III) OXIDATION; WATER OXIDATION; HEXAGONAL BIRNESSITE;
MULTIPLET STRUCTURE; CR(III) OXIDATION; RIETVELD REFINEMENT; XANES
SPECTROSCOPY
AB Hydrous manganese oxides are an important class of minerals that help regulate the geochemical redox cycle in near-surface environments and are also considered to be promising catalysts for energy applications such as the oxidation of water. A complete characterization of these minerals is required to better understand their catalytic and redox activity. In this contribution an empirical methodology using X-ray photoelectron spectroscopy (XPS) is developed to quantify the oxidation state of hydrous multivalent manganese oxides with an emphasis on birnessite, a layered structure that occurs commonly in soils but is also the oxidized endmember in biomimetic water-oxidation catalysts. The Mn2p(3/2), Mn3p, and Mn3s lines of near monovalent Mn(II), Mn(III), and Mn(IV) oxides were fit with component peaks; after the best fit was obtained the relative widths, heights and binding energies of the components were fixed. Unknown multivalent samples were fit such that binding energies, intensities, and peak-widths of each oxidation state, composed of a packet of correlated component peaks, were allowed to vary. Peak-widths were constrained to maintain the difference between the standards. Both average and individual mole fraction oxidation states for all three energy levels were strongly correlated, with close agreement between Mn3s and Mn3p analyses, whereas calculations based on the Mn2p(3/2) spectra gave systematically more reduced results. Limited stoichiometric analyses were consistent with Mn3p and Mn3s. Further, evidence indicates the shape of the Mn3p line was less sensitive to the bonding environment than that for Mn2p. Consequently, fitting the Mn3p and Mn3s lines yielded robust quantification of oxidation states over a range of Mn (hydr)oxide phases. In contrast, a common method for determining oxidation states that utilizes the multiplet splitting of the Mn3s line was found to be not appropriate for birnessites. (C) 2016 Published by Elsevier B.V.
C1 [Ilton, Eugene S.; Kerisit, Sebastien N.] Pacific NW Natl Lab, 902 Battelle Blvd, Richland, WA 99352 USA.
[Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, NHB 119,POB 37012, Washington, DC 20013 USA.
[Heaney, Peter J.; Ling, Florence T.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Ilton, ES (reprint author), Pacific NW Natl Lab, 902 Battelle Blvd, Richland, WA 99352 USA.
EM eugene.ilton@pnnl.gov
OI Ling, Florence/0000-0002-2576-3608
FU U.S. Department of Energy (DOE), Office of Basic Energy Sciences,
Division of Chemical Sciences, Geosciences Biosciences; U.S. DOE's
Office of Biological and Environmental Research; DOE by Battelle
Memorial Institute [DE-AC06-76RLO-1830]; NSF [EAR11-47728]
FX ESI and SNK were supported by the PNNL managed Geosciences Research
Program of the U.S. Department of Energy (DOE), Office of Basic Energy
Sciences, Division of Chemical Sciences, Geosciences & Biosciences. The
research was performed in part using the Environmental Molecular
Sciences Laboratory (EMSL), a national scientific user facility
sponsored by the U.S. DOE's Office of Biological and Environmental
Research and located at Pacific Northwest National Laboratory (PNNL).
PNNL is operated for DOE by Battelle Memorial Institute under Contract#
DE-AC06-76RLO-1830. We also acknowledge support from NSF EAR11-47728. We
thank Paul Bagus for comments on an earlier version of the manuscript
and both Manjula Nandasiri and Ashleigh Schwarz for operating the XPS
facility. Comments by two anonymous reviewers are greatly appreciated.
NR 64
TC 10
Z9 10
U1 37
U2 82
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
EI 1873-5584
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD MAR 15
PY 2016
VL 366
BP 475
EP 485
DI 10.1016/j.apsusc.2015.12.159
PG 11
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA DH1AT
UT WOS:000372517500058
ER
PT J
AU Le Roux, JP
Achurra, L
Henriquez, A
Carreno, C
Rivera, H
Suarez, ME
Ishman, SE
Pyenson, ND
Gutstein, CS
AF Le Roux, Jacobus P.
Achurra, Luciano
Henriquez, Alvaro
Carreno, Catalina
Rivera, Huber
Suarez, Mario E.
Ishman, Scott E.
Pyenson, Nicholas D.
Gutstein, Carolina S.
TI Oroclinal bending of the Juan Fernandez Ridge suggested by geohistory
analysis of the Bahia Inglesa Formation, north-central Chile
SO SEDIMENTARY GEOLOGY
LA English
DT Article
DE Rocky shoreline deposits; Tsunami deposits; Juan Fernandez Ridge;
Copiapo Ridge; Copiapo ignimbrite; Bulimina marginata
ID SOUTHERN CENTRAL ANDES; MIDDLE MIOCENE AGE; SEA-LEVEL CHANGES; ET-AL.
2013; NAVIDAD FORMATION; TECTONIC IMPLICATIONS; SUBDUCTION EROSION;
FORE-ARC; SEDIMENTARY STRUCTURES; COQUIMBO FORMATION
AB The stratigraphy of the Bahia Inglesa Formation in the Caldera Basin west of Copiapo, (north-central Chile) is revised, based on hitherto unpublished stratigraphic sections and Sr-87/Sr-86 dating. The depositional environment varied from a rocky shoreline to the upper continental slope, with sea-level oscillations and tectonic movements causing numerous local unconformities as well as lateral and vertical fades changes. Geohistory and sedimentological analyses show that the area was close to the concurrent sea level at about 15.3 Ma, but at the same time being elevated about 100 m above the present sea level. Although the basin then subsided at least 350 m until around 6 Ma, marine deposition was only recorded after 10.4 Ma. This suggests that the sea level initially dropped faster than the rate of subsidence so that subaerial erosion occurred. The period of subaerial exposure before 10.4 Ma can be attributed to the presence of a NE-trending branch of the Juan Fernandez Ridge below the continental crust at this time, whereas the ensuing subsidence was due to subduction erosion and crustal accommodation in its wake as it migrated south along the South American coastline. The subsequent uplift of at least 250 m can be explained by an acceleration in plate expansion and isostatic rebound of the continental crust after being partially submerged in the upper mantle. The uplift-subsidence-uplift pattern mirrors those recorded around the Nazca Ridge in Peru, as well as in similar basins to the south of Caldera. However, a higher southward migration rate of the Juan Fernandez Ridge against the edge of the South American Plate and less intense uplift subsidence-uplift cycles are recorded in the latter basins. This can possibly be attributed to oroclinal bending of the ridge due to friction with the overlying continental plate, which diminished the angle of incidence and the intensity of the stress field, but increased the migration velocity of the ridge relative to the coastline. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Le Roux, Jacobus P.; Rivera, Huber] Univ Chile, Dept Geol, Fac Ciencias Fis & Matemat, Plaza Ercilla 803, Santiago, Chile.
[Le Roux, Jacobus P.] Andean Geothermal Ctr Excellence, Plaza Ercilla 803, Santiago, Chile.
[Achurra, Luciano] Arcadis Consultores, Santiago, Chile.
[Henriquez, Alvaro] SQM SA, Calama, Chile.
[Carreno, Catalina] Corp Nacl Cobre, Calama, Chile.
[Suarez, Mario E.] Univ Chile, Fac Ciencias, Lab Ontogenia & Filogenia, Santiago, Chile.
[Ishman, Scott E.] So Illinois Univ, Dept Geol, Carbondale, IL 62901 USA.
[Pyenson, Nicholas D.; Gutstein, Carolina S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
[Pyenson, Nicholas D.; Gutstein, Carolina S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, POB 37012, Washington, DC 20013 USA.
[Gutstein, Carolina S.] Consejo Monumentos Nacl, Comis Patrimonio Nat, Av Vicuna Mackenna 84, Santiago, Chile.
RP Le Roux, JP (reprint author), Univ Chile, Dept Geol, Plaza Ercilla 803, Santiago, Chile.
EM jroux@cec.uchile.cl
RI Le Roux, Jacobus/A-9765-2008
OI Le Roux, Jacobus/0000-0003-0173-4471
FU Project Fondecyt [1010691, 130006]; Project National Geographic Society
Committee on Research Exploration [8903-11, 9019-11]; Project
CONICYT/FONDAP [15090013]
FX The authors are greatly indebted to financial and logistical support
from Projects Fondecyt 1010691 and 130006, National Geographic Society
Committee on Research Exploration grants 8903-11 and 9019-11, and
Project CONICYT/FONDAP 15090013. Two anonymous reviewers are thanked for
their critical but very constructive comments.
NR 101
TC 0
Z9 0
U1 1
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0037-0738
EI 1879-0968
J9 SEDIMENT GEOL
JI Sediment. Geol.
PD MAR 15
PY 2016
VL 333
BP 32
EP 49
DI 10.1016/j.sedgeo.2015.12.003
PG 18
WC Geology
SC Geology
GA DF9AT
UT WOS:000371653300003
ER
PT J
AU Daubar, IJ
Dundas, CM
Byrne, S
Geissler, P
Bart, GD
McEwen, AS
Russell, PS
Chojnacki, M
Golombek, MP
AF Daubar, I. J.
Dundas, C. M.
Byrne, S.
Geissler, P.
Bart, G. D.
McEwen, A. S.
Russell, P. S.
Chojnacki, M.
Golombek, M. P.
TI Changes in blast zone albedo patterns around new martian impact craters
SO ICARUS
LA English
DT Article
DE Impact processes; Aeolian processes; Cratering; Mars; Mars, surface
ID SCIENCE EXPERIMENT HIRISE; MARS ORBITER CAMERA; SLOPE STREAKS;
LUNAR-SURFACE; STRUCTURAL DISTURBANCES; DUST; EXPLORATION; SPACECRAFT
AB "Blast zones" (BZs) around new martian craters comprise various albedo features caused by the initial impact, including diffuse halos, extended linear and arcuate rays, secondary craters, ejecta patterns, and dust avalanches. We examined these features for changes in repeat images separated by up to four Mars years. Here we present the first comprehensive survey of the qualitative and quantitative changes observed in impact blast zones over time. Such changes are most likely due to airfall of high-albedo dust restoring darkened areas to their original albedo, the albedo of adjacent non-impacted surfaces. Although some sites show drastic changes over short timescales, nearly half of the sites show no obvious changes over several Mars years. Albedo changes are more likely to occur at higher-latitude sites, lower-elevation sites, and at sites with smaller central craters. No correlation was seen between amount of change and Dust Cover Index, relative halo size, or historical regional albedo changes. Quantitative albedo measurements of the diffuse dark halos relative to their surroundings yielded estimates of fading lifetimes for these features. The average lifetime among sites with measurable fading is similar to 15 Mars years; the median is similar to 8 Mars years for a linear brightening. However, at approximately half of sites with three or more repeat images, a nonlinear function with rapid initial fading followed by a slow increase in albedo provides a better fit to the fading behavior; this would predict even longer lifetimes. The predicted lifetimes of BZs are comparable to those of slope streaks, and considered representative of fading by global atmospheric dust deposition; they last significantly longer than dust devil or rover tracks, albedo features that are erased by different processes. These relatively long lifetimes indicate that the measurement of the current impact rate by Daubar et al. (Daubar, I.J. et al. [2013]. Icarus 225, 506-516. http://dx.doi.org/ 10.1016/j.icarus.2013.04.009) does not suffer significantly from overall under-sampling due to blast zones fading before new impact sites can be initially discovered. However, the prevalence of changes seen around smaller craters may explain in part their shallower size frequency distribution. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Daubar, I. J.; Golombek, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Daubar, I. J.; Byrne, S.; McEwen, A. S.; Chojnacki, M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Dundas, C. M.; Geissler, P.] US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA.
[Bart, G. D.] Univ Idaho, Dept Phys, 875 Perimeter Dr,MS 0903, Moscow, ID 83843 USA.
[Russell, P. S.] Natl Air & Space Museum, Smithsonian Inst, MRC 315,POB 37012, Washington, DC 20013 USA.
RP Daubar, IJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM ingrid.daubar@jpl.nasa.gov
RI Chojnacki, Matthew/A-4245-2013;
OI Chojnacki, Matthew/0000-0001-8497-8994; Dundas,
Colin/0000-0003-2343-7224
FU National Aeronautics and Space Administration
FX We are grateful for the HiRISE operations staff for acquiring and
processing the excellent data used in this study, and the CTX operations
team for discovering candidate new impact sites. Our thanks go to Rod
Heyd for answering questions about the detailed processing of HiRISE
RDRs and Guy McArthur for help with the HiView software. Patricio
Becerra also provided useful discussion. We appreciate the helpful
comments from Moses Milazzo and two anonymous reviewers, especially one
reviewer whose thoughtful and detailed comments greatly improved this
work. This work was partially supported by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology, administered by Oak Ridge Associated
Universities through a contract with the National Aeronautics and Space
Administration.
NR 64
TC 5
Z9 5
U1 1
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 86
EP 105
DI 10.1016/j.icarus.2015.11.032
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700008
ER
PT J
AU Norrbom, AL
Savaris, M
Marinoni, L
AF Norrbom, Allen L.
Savaris, Marcoandre
Marinoni, Luciane
TI New species of Rhagoletotrypeta (Diptera: Tephritidae) from the
Dominican Republic and southern Brazil and Paraguay
SO ZOOTAXA
LA English
DT Article
DE fruit flies; taxonomy; host plant; Celtis
AB Rhagoletotrypeta chapecensis Norrbom & Savaris, new species, and R. gelabertae Norrbom & Savaris, new species, are described and illustrated from specimens from southern Brazil (Parana, Santa Catarina) and Paraguay, and from the Dominican Republic, respectively. The larvae of R. chapecensis develop in fruits of Celtis iguanaea (Jacq.) Sarg. (Ulmaceae). A key to the species of the xanthogastra species group is provided.
C1 [Norrbom, Allen L.] USDA ARS, Smithsonian Inst, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA.
[Savaris, Marcoandre; Marinoni, Luciane] Univ Fed Parana, Dept Zool, Jardim Amer, BR-81531980 Curitiba, Parana, Brazil.
RP Norrbom, AL (reprint author), USDA ARS, Smithsonian Inst, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA.; Savaris, M; Marinoni, L (reprint author), Univ Fed Parana, Dept Zool, Jardim Amer, BR-81531980 Curitiba, Parana, Brazil.
EM allen.norrbom@ars.usda.gov; plaumannimyia@gmail.com; lmarinoni@ufpr.br
RI Marinoni, Luciane /C-5720-2013
FU CNPq [200277/2015-4]
FX We thank Lucrecia Rodriguez for assistance with the illustrations. CNPq
provided financial support for MS and LM (Process number 200277/2015-4).
USDA is an equal opportunity provider and employer.
NR 8
TC 0
Z9 0
U1 0
U2 1
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD MAR 11
PY 2016
VL 4088
IS 4
BP 547
EP 554
PG 8
WC Zoology
SC Zoology
GA DH4UF
UT WOS:000372780200005
PM 27394357
ER
PT J
AU Earnshaw, HM
Roberts, TP
Heil, LM
Mezcua, M
Walton, DJ
Done, C
Harrison, FA
Lansbury, GB
Middleton, MJ
Sutton, AD
AF Earnshaw, Hannah M.
Roberts, Timothy P.
Heil, Lucy M.
Mezcua, Mar
Walton, Dominic J.
Done, Chris
Harrison, Fiona A.
Lansbury, George B.
Middleton, Matthew J.
Sutton, Andrew D.
TI A variable ULX and possible IMBH candidate in M51a
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: black holes; black hole physics;
galaxies: individual: M51; X-rays: binaries; X-rays: individual: M51
ULX-7
ID X-RAY SOURCES; MASS BLACK-HOLE; XMM-NEWTON OBSERVATIONS; ESO 243-49
HLX-1; SPECTRAL STATE TRANSITIONS; ACTIVE GALACTIC NUCLEI; NGC 5408 X-1;
OPTICAL COUNTERPARTS; SPIRAL-GALAXIES; ULTRALUMINOUS STATE
AB Ultraluminous X-ray source (ULX)-7, in the northern spiral arm of M51, demonstrates unusual behaviour for an ULX, with a hard X-ray spectrum but very high short-term variability. This suggests that it is not in a typical ultraluminous state. We analyse the source using archival data from XMM-Newton, Chandra and NuSTAR, and by examining optical and radio data from HST and Very Large Array. Our X-ray spectral analysis shows that the source has a hard power-law spectral shape with a photon index Gamma similar to 1.5, which persists despite the source's X-ray luminosity varying by over an order of magnitude. The power spectrum of the source features a break at 6.5(-1.1)(+0.5) x 10(-3) Hz, from a low-frequency spectral index of alpha(1) = -0.1(-0.2)(+0.5) to a high-frequency spectral index of alpha(2) = 6.5(-0.14)(+0.05), making it analogous to the low-frequency break found in the power spectra of low/hard state black holes (BHs). We can take a lower frequency limit for a corresponding high-frequency break to calculate a BH mass upper limit of 1.6 x 10(3) M-circle dot. Using the X-ray/radio Fundamental Plane, we calculate another upper limit to the BH mass of 3.5 x 10(4) M-circle dot for a BH in the low/hard state. The hard spectrum, high rms variability and mass limits are consistent with ULX-7 being an intermediate-mass BH; however we cannot exclude other interpretations of this source's interesting behaviour, most notably a neutron star with an extreme accretion rate.
C1 [Earnshaw, Hannah M.; Roberts, Timothy P.; Done, Chris; Lansbury, George B.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Heil, Lucy M.] Anton Pannekoek Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Mezcua, Mar] Univ Montreal, Pavillon Roger Gaudry D-428, Montreal, PQ H3T 1J4, Canada.
[Mezcua, Mar] Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
[Walton, Dominic J.; Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA.
[Middleton, Matthew J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Sutton, Andrew D.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA.
RP Earnshaw, HM (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
EM hannah.earnshaw@durham.ac.uk
OI Earnshaw, Hannah P/0000-0001-5857-5622
FU Science and Technology Facilities Council [ST/K501979/1, ST/L00075X/1];
NASA [G05-16099X]; ESA Member States
FX We gratefully acknowledge support from the Science and Technology
Facilities Council (HE through grant ST/K501979/1 and TR as part of
consolidated grant ST/L00075X/1) and from NASA (MM through Chandra Grant
G05-16099X). AS is supported by an appointment to the NASA Postdoctoral
Program at Marshall Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA.; The scientific
results reported in this paper are based on data obtained from the
Chandra Data Archive, and on archival observations obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. This research has also
made use of data obtained with NuSTAR, a project led by Caltech, funded
by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software
package, jointly developed by the ASDC (Italy) and Caltech (USA).
Further results are based on observations made with the NASA/ESA HST,
and obtained from the Hubble Legacy Archive, which is a collaboration
between the Space Telescope Science Institute (STScI/NASA), the Space
Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian
Astronomy Data Centre (CADC/NRC/CSA); and the National Radio Astronomy
Observatory, which is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 85
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3840
EP 3854
DI 10.1093/mnras/stv2945
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800032
ER
PT J
AU Sadowski, A
Lasota, JP
Abramowicz, MA
Narayan, R
AF Sadowski, Aleksander
Lasota, Jean-Pierre
Abramowicz, Marek A.
Narayan, Ramesh
TI Energy flows in thick accretion discs and their consequences for black
hole feedback
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; relativistic processes;
methods: numerical
ID ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; MAGNETIC-FLUX;
RELATIVISTIC MAGNETOHYDRODYNAMICS; ELECTROMAGNETIC EXTRACTION;
DIFFUSION-COEFFICIENTS; NUMERICAL-SIMULATION; GENERAL-RELATIVITY;
VERTICAL STRUCTURE; DISKS
AB We study energy flows in geometrically thick accretion discs, both optically thick and thin, using general relativistic, three-dimensional simulations of black hole accretion flows. We find that for non-rotating black holes the efficiency of the total feedback from thick accretion discs is 3 per cent - roughly half of the thin disc efficiency. This amount of energy is ultimately distributed between outflow and radiation, the latter scaling weakly with the accretion rate for super-critical accretion rates, and returned to the interstellar medium. Accretion on to rotating black holes is more efficient because of the additional extraction of rotational energy. However, the jet component is collimated and likely to interact only weakly with the environment, whereas the outflow and radiation components cover a wide solid angle.
C1 [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Lasota, Jean-Pierre] CNRS, Inst Astrophys Paris, 98Bis Bd Arago, F-75014 Paris, France.
[Lasota, Jean-Pierre] Univ Paris 06, Sorbonne Univ, UMR 7095, 98Bis Bd Arago, F-75014 Paris, France.
[Lasota, Jean-Pierre; Abramowicz, Marek A.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
[Abramowicz, Marek A.] Gothenburg Univ, Dept Phys, SE-41296 Gothenburg, Sweden.
[Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA.
RP Sadowski, A (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM asadowsk@mit.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA through Einstein Postdoctoral Fellowship by the Chandra X-ray
Center [PF4-150126]; NASA [NAS8-03060, TCAN NNX14AB47G]; Polish NCN
grant [UMO-2013/08/A/ST9/00795, DEC-2012/04/A/ST9/00083]; French Space
Agency CNES; NSF [AST1312651]; NSF via XSEDE resources [TG-AST080026N];
NASA via the High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center
FX AS acknowledges support for this work by NASA through Einstein
Postdoctoral Fellowship number PF4-150126 awarded by the Chandra X-ray
Center, which is operated by the Smithsonian Astrophysical Observatory
for NASA under contract NAS8-03060. AS thanks Harvard-Smithsonian Center
for Astrophysics for its hospitality. This research was supported by the
Polish NCN grants UMO-2013/08/A/ST9/00795 and DEC-2012/04/A/ST9/00083.
JPL was supported in part by a grant from the French Space Agency CNES.
RN was supported in part by NSF grant AST1312651 and NASA grant TCAN
NNX14AB47G. The authors acknowledge computational support from NSF via
XSEDE resources (grant TG-AST080026N) and from NASA via the High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center.
NR 64
TC 7
Z9 7
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3915
EP 3928
DI 10.1093/mnras/stv2854
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800037
ER
PT J
AU Sadowski, A
Narayan, R
AF Sadowski, Aleksander
Narayan, Ramesh
TI Three-dimensional simulations of supercritical black hole accretion
discs - luminosities, photon trapping and variability
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; relativistic processes;
methods: numerical
ID RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS; SUPER-EDDINGTON ACCRETION;
RELATIVISTIC MAGNETOHYDRODYNAMICS; NUMERICAL SIMULATIONS;
GENERAL-RELATIVITY; THICK ACCRETION; M1 CLOSURE; FLOWS; DISKS; SPECTRA
AB We present a set of four three-dimensional, general relativistic, radiation magnetohydrodynamical simulations of black hole accretion at supercritical mass accretion rates, (M) over dot > (M) over dot(Edd). We use these simulations to study how disc properties are modified when we vary the black hole mass, the black hole spin, or the mass accretion rate. In the case of a non-rotating black hole, we find that the total efficiency is of the order of 3 per cent (M) over dotc(2), approximately a factor of 2 less than the efficiency of a standard thin accretion disc. The radiation flux in the funnel along the axis is highly super-Eddington, but only a small fraction of the energy released by accretion escapes in this region. The bulk of the 3 per cent (M) over dotc(2) of energy emerges farther out in the disc, either in the form of photospheric emission or as a wind. In the case of a black hole with a spin parameter of 0.7, we find a larger efficiency of about 8 per cent (M) over dotc(2). By comparing the relative importance of advective and diffusive radiation transport, we show that photon trapping is effective near the equatorial plane. However, near the disc surface, vertical transport of radiation by diffusion dominates. We compare the properties of our fiducial three-dimensional run with those of an equivalent two-dimensional axisymmetric model with a mean-field dynamo. The latter simulation runs nearly 100 times faster than the three-dimensional simulation, and gives very similar results for time-averaged properties of the accretion flow, but does not reproduce the time-variability.
C1 [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA.
RP Sadowski, A (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM asadowsk@mit.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA through Einstein Postdoctotral Fellowship by the Chandra X-ray
Center [PF4-150126]; NASA [NAS8-03060, TCAN NNX14AB47G]; NSF
[AST1312651]; NSF via XSEDE resources [TG-AST080026N]
FX The authors thank Jean-Pierre Lasota and Jonathan McKinney for their
comments. AS acknowledges support for this work by NASA through Einstein
Postdoctotral Fellowship number PF4-150126 awarded by the Chandra X-ray
Center, which is operated by the Smithsonian Astrophysical Observatory
for NASA under contract NAS8-03060. AS thanks Harvard-Smithsonian Center
for Astrophysics for hospitality. RN was supported in part by NSF grant
AST1312651 and NASA grant TCAN NNX14AB47G. The authors acknowledge
computational support from NSF via XSEDE resources (grant
TG-AST080026N), and from NASA via the High-End Computing (HEC) Program
through the NASA Advanced Supercomputing (NAS) Division at Ames Research
Center.
NR 49
TC 15
Z9 15
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3929
EP 3947
DI 10.1093/mnras/stv2941
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800038
ER
PT J
AU Siwak, M
Ogloza, W
Rucinski, SM
Moffat, AFJ
Matthews, JM
Cameron, C
Guenther, DB
Kuschnig, R
Rowe, JF
Sasselov, D
Weiss, WW
AF Siwak, Michal
Ogloza, Waldemar
Rucinski, Slavek M.
Moffat, Anthony F. J.
Matthews, Jaymie M.
Cameron, Chris
Guenther, David B.
Kuschnig, Rainer
Rowe, Jason F.
Sasselov, Dimitar
Weiss, Werner W.
TI Stable and unstable accretion in the classical T Tauri stars IM Lup and
RU Lup as observed by MOST
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: RULup; stars: individual:
IMLup; stars: rotation; stars: variables: T Tauri, Herbig Ae/Be
ID MAIN-SEQUENCE STARS; QUASI-PERIODIC OSCILLATIONS; LIMB-DARKENING
COEFFICIENTS; RADIAL-VELOCITY; PHOTOMETRIC VARIABILITY; DISK ACCRETION;
LIGHT CURVES; YOUNG STARS; MAGNETOHYDRODYNAMIC SIMULATIONS; BROADENING
FUNCTIONS
AB Results of the time variability monitoring of the two classical T Tauri stars, RU Lup and IM Lup, are presented. Three photometric data sets were utilized: (1) simultaneous (same field) MOST satellite observations over four weeks in each of the years 2012 and 2013, (2) multicolour observations at the South African Astronomical Observatory in April-May of 2013, (3) archival V-filter All Sky Automated Survey (ASAS) data for nine seasons, 2001-2009. They were augmented by an analysis of high-resolution, public-domain VLT-UT2 Ultraviolet Visual Echelle Spectrograph spectra from the years 2000 to 2012. From the MOST observations, we infer that irregular light variations of RU Lup are caused by stochastic variability of hotspots induced by unstable accretion. In contrast, the MOST light curves of IM Lup are fairly regular and modulated with a period of about 7.19-7.58 d, which is in accord with ASAS observations showing a well-defined 7.247 +/- 0.026 d periodicity. We propose that this is the rotational period of IM Lup and is due to the changing visibility of two antipodal hotspots created near the stellar magnetic poles during the stable process of accretion. Re-analysis of RU Lup high-resolution spectra with the broadening function approach reveals signs of a large polar coldspot, which is fairly stable over 13 years. As the star rotates, the spot-induced depression of intensity in the broadening function profiles changes cyclically with period 3.710 58 d, which was previously found by the spectral cross-correlation method.
C1 [Siwak, Michal; Ogloza, Waldemar] Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland.
[Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada.
[Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, 1250 Grand Lake Rd, Sydney, NS B1P 6L2, Canada.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland.
EM siwak@nac.oa.uj.edu.pl
FU ESO Science Archive Facility [65.I-0404, 69.C-0481, 075.C-0292,
081.C-0779, 089.C-0299]; Polish National Science Centre
[2012/05/E/ST9/03915]; Natural Sciences and Engineering Research Council
of Canada; FRQNT (Quebec); Canadian Space Agency; Austrian Science Funds
[P22691-N16]
FX This study was based on the following:; (1) data from the MOST
satellite, a Canadian Space Agency mission jointly operated by Dynacon
Inc., the University of Toronto Institute of Aerospace Studies and the
University of British Columbia, with the assistance of the University of
Vienna,; (2) observations made at the South African Astronomical
Observatory,; (3) data obtained from the ESO Science Archive Facility
under request numbers 145841 and 145843, within the programmes ID
65.I-0404, 69.C-0481, 075.C-0292, 081.C-0779 and 089.C-0299,; (4) data
obtained from the All Sky Automated Survey (ASAS) telescope of the
Warsaw University Astronomical Observatory.; MS and WO are grateful to
the Polish National Science Centre for the grant 2012/05/E/ST9/03915.
The Natural Sciences and Engineering Research Council of Canada supports
the research of DBG, JMM, AFJM and SMR. Additional support for AFJM was
provided by FRQNT (Quebec). CC was supported by the Canadian Space
Agency. RK and WWW are supported by the Austrian Science Funds
(P22691-N16). MS and WO acknowledge Dr Hannah Worters and the entire
SAAO staff for their hospitality.
NR 84
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3972
EP 3984
DI 10.1093/mnras/stv2848
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800042
ER
PT J
AU Castillo, GAR
Israel, GL
Tiengo, A
Salvetti, D
Turolla, R
Zane, S
Rea, N
Esposito, P
Mereghetti, S
Perna, R
Stella, L
Pons, JA
Campana, S
Gotz, D
Motta, S
AF Castillo, Guillermo A. Rodriguez
Israel, Gian Luca
Tiengo, Andrea
Salvetti, David
Turolla, Roberto
Zane, Silvia
Rea, Nanda
Esposito, Paolo
Mereghetti, Sandro
Perna, Rosalba
Stella, Luigi
Pons, Jose A.
Campana, Sergio
Goetz, Diego
Motta, Sara
TI The outburst decay of the low magnetic field magnetar SWIFT
J1822.3-1606: phase-resolved analysis and evidence for a variable
cyclotron feature
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: SWIFT J1822.3-16066; stars: magnetar; stars: neutron;
X-rays: bursts
ID X-RAY PULSARS; NEUTRON-STARS; 3XMM J185246.6+003317; TRANSIENT MAGNETAR;
ABSORPTION FEATURE; XTE J1810-197; SGR 0418+5729; ABUNDANCES; DISCOVERY;
MODEL
AB We study the timing and spectral properties of the low-magnetic field, transient magnetar SWIFT J1822.3-1606 as it approached quiescence. We coherently phase-connect the observations over a time-span of similar to 500 d since the discovery of SWIFT J1822.3-1606 following the Swift-Burst Alert Telescope (BAT) trigger on 2011 July 14, and carried out a detailed pulse phase spectroscopy along the outburst decay. We follow the spectral evolution of different pulse phase intervals and find a phase and energy-variable spectral feature, which we interpret as proton cyclotron resonant scattering of soft photon from currents circulating in a strong (greater than or similar to 10(14) G) small-scale component of the magnetic field near the neutron star surface, superimposed to the much weaker (similar to 3 x 10(13) G) magnetic field. We discuss also the implications of the pulse-resolved spectral analysis for the emission regions on the surface of the cooling magnetar.
C1 [Castillo, Guillermo A. Rodriguez; Israel, Gian Luca; Stella, Luigi] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Castillo, Guillermo A. Rodriguez] Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
[Tiengo, Andrea; Salvetti, David; Esposito, Paolo; Mereghetti, Sandro] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy.
[Tiengo, Andrea] Ist Univ Studi Superiori, Piazza Vittoria 15, I-27100 Pavia, Italy.
[Tiengo, Andrea] Ist Nazl Fis Nucl, Sez Pavia, Via V Bassi 6, I-27100 Pavia, Italy.
[Turolla, Roberto] Univ Padua, Dipartimento Fis & Astron, Via Marzolo 8, I-35131 Padua, Italy.
[Turolla, Roberto; Zane, Silvia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Rea, Nanda] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Rea, Nanda] Inst Space Sci CSIC IEEC, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain.
[Esposito, Paolo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Perna, Rosalba] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Pons, Jose A.] Univ Alacant, Dept Fis Aplicada, E-03080 Alacant, Spain.
[Campana, Sergio] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy.
[Goetz, Diego] Univ Paris Diderot, CNRS, CEA, AIM,Irfu,Serv Astrophys Saclay,DSM, F-91191 Gif Sur Yvette, France.
[Motta, Sara] European Space Astron Ctr, E-28692 Madrid, Spain.
RP Castillo, GAR (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.; Castillo, GAR (reprint author), Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
EM grodriguez-cas@gmail.com
RI PONS, JOSE/D-4687-2012;
OI PONS, JOSE/0000-0003-1018-8126; Rodriguez Castillo, Guillermo
Andres/0000-0003-3952-7291; Esposito, Paolo/0000-0003-4849-5092; Rea,
Nanda/0000-0003-2177-6388
NR 31
TC 3
Z9 3
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 4145
EP 4155
DI 10.1093/mnras/stv2490
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800057
ER
PT J
AU Kitaura, FS
Rodriguez-Torres, S
Chuang, CH
Zhao, C
Prada, F
Gil-Marin, H
Guo, H
Yepes, G
Klypin, A
Scoccola, CG
Tinker, J
McBride, C
Reid, B
Sanchez, AG
Salazar-Albornoz, S
Grieb, JN
Vargas-Magana, M
Cuesta, AJ
Neyrinck, M
Beutler, F
Comparat, J
Percival, WJ
Ross, A
AF Kitaura, Francisco-Shu
Rodriguez-Torres, Sergio
Chuang, Chia-Hsun
Zhao, Cheng
Prada, Francisco
Gil-Marin, Hector
Guo, Hong
Yepes, Gustavo
Klypin, Anatoly
Scoccola, Claudia G.
Tinker, Jeremy
McBride, Cameron
Reid, Beth
Sanchez, Ariel G.
Salazar-Albornoz, Salvador
Grieb, Jan Niklas
Vargas-Magana, Mariana
Cuesta, Antonio J.
Neyrinck, Mark
Beutler, Florian
Comparat, Johan
Percival, Will J.
Ross, Ashley
TI The clustering of galaxies in the SDSS-III Baryon Oscillation
Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data
Release
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; galaxies: haloes; galaxies: statistics; large-scale
structure of Universe
ID LARGE-SCALE STRUCTURE; COLD DARK-MATTER; HALO OCCUPATION DISTRIBUTION;
DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; N-BODY SIMULATIONS;
ACOUSTIC-OSCILLATIONS; POWER-SPECTRUM; LAMBDA-CDM; PERTURBATION-THEORY
AB We reproduce the galaxy clustering catalogue from the SDSS-III Baryon Oscillation Spectroscopic Survey Final Data Release (BOSS DR11&DR12) with high fidelity on all relevant scales in order to allow a robust analysis of baryon acoustic oscillations and redshift space distortions. We have generated (6000) 12 288 MultiDark PATCHY BOSS (DR11) DR12 light cones corresponding to an effective volume of similar to 192 000 [h(-1) Gpc](3) (the largest ever simulated volume), including cosmic evolution in the redshift range from 0.15 to 0.75. The mocks have been calibrated using a reference galaxy catalogue based on the halo abundance matching modelling of the BOSS DR11&DR12 galaxy clustering data and on the data themselves. The production follows three steps. First, we apply the PATCHY code to generate a dark matter field and an object distribution including non-linear stochastic galaxy bias. Secondly, we run the halo/stellar distribution reconstruction HADRON code to assign masses to the various objects. This step uses the mass distribution as a function of local density and non-local indicators (i.e. tidal field tensor eigenvalues and relative halo exclusion separation for massive objects) from the reference simulation applied to the corresponding patchy dark matter and galaxy distribution. Finally, we apply the SUGAR code to build the light cones. The resulting MultiDarkPATCHY mock light cones reproduce the number density, selection function, survey geometry, and in general within 1 sigma, for arbitrary stellar mass bins, the power spectrum up to k = 0.3 h Mpc(-1), the two-point correlation functions down to a few Mpc scales, and the three-point statistics of the BOSS DR11&DR12 galaxy samples.
C1 [Kitaura, Francisco-Shu] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Rodriguez-Torres, Sergio; Chuang, Chia-Hsun; Prada, Francisco; Comparat, Johan] Univ Autonoma Madrid, UAM CSIC, Inst Fis Teor, E-28049 Madrid, Spain.
[Rodriguez-Torres, Sergio; Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain.
[Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Zhao, Cheng] Tsinghua Univ, Tsinghua Ctr Astrophys, Dept Phys, Beijing 100084, Peoples R China.
[Prada, Francisco] Inst Astrofis Andalucia CSIC, Glorieta Astron, E-18080 Granada, Spain.
[Gil-Marin, Hector; Percival, Will J.; Ross, Ashley] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England.
[Guo, Hong] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China.
[Guo, Hong] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Klypin, Anatoly] New Mexico State Univ, Astron Dept, Las Cruces, NM 88003 USA.
[Klypin, Anatoly] Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain.
[Scoccola, Claudia G.] Inst Astrofis Canarias IAC, C Via Lactea S-N, E-38200 Tenerife, Spain.
[Scoccola, Claudia G.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Tinker, Jeremy] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[McBride, Cameron] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Reid, Beth; Beutler, Florian] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd,Berkeley, Berkeley, CA 94720 USA.
[Reid, Beth] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Reid, Beth] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Sanchez, Ariel G.; Salazar-Albornoz, Salvador; Grieb, Jan Niklas] Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany.
[Salazar-Albornoz, Salvador; Grieb, Jan Niklas] Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Apdo Postal 20-364, Mexico City 01000, DF, Mexico.
[Cuesta, Antonio J.; Neyrinck, Mark] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain.
[Neyrinck, Mark] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ross, Ashley] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
RP Kitaura, FS (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
EM kitaura@aip.de
RI Guo, Hong/J-5797-2015; Gil Marin, Hector/B-2013-2017;
OI Guo, Hong/0000-0003-4936-8247; Gil Marin, Hector/0000-0003-0265-6217;
Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio
Jose/0000-0002-4153-9470
FU Spanish MICINNs Consolider-Ingenio Programme under grant MultiDark
[CSD2009-00064]; MINECO Centro de Excelencia Severo Ochoa Programme
[SEV-2012-0249, AYA2014-60641-C2-1-P]; Spanish MEC 'Salvador de
Madariaga' programme [PRX14/00444]; UK Science and Technology Facilities
Council [ST/I001204/1]; Chinese Academy of Sciences; MINECO (Spain)
[AYA2012-31101, FPA2012-34694]; Transregional Collaborative Research
Centre TR33 'The Dark Universe' of the German Research Foundation (DFG);
European Research Council under the European Community
[FP7-IDEAS-Phys.LSS 240117]; Spanish MINECO of ICCUB (Unidad de
Excelencia 'Maria de Maeztu') [MDM-2014-0369]; ICG; SEPNet; University
of Portsmouth; Office of Science of the US Department of Energy
[DE-AC02-05CH11231]; Alfred P. Sloan Foundation; National Science
Foundation; US Department of Energy Office of Science; University of
Arizona; Brazilian Participation Group; Brookhaven National Laboratory;
University of Cambridge; Carnegie Mellon University; University of
Florida; French Participation Group; German Participation Group; Harvard
University; Instituto de Astrofisica de Canarias; Michigan State/Notre
Dame/JINA Participation Group; Johns Hopkins University; Lawrence
Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max
Planck Institute for Extraterrestrial Physics; New Mexico State
University; New York University; Ohio State University; Pennsylvania
State University; Princeton University; Spanish Participation Group;
University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; University of Washington; Yale University;
[2012060963]
FX FSK, SRT, CC, CZ, FP, AK, and CGS acknowledge support from the Spanish
MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark
CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under
grant SEV-2012-0249, and grant AYA2014-60641-C2-1-P. FSK and CZ also
want to thank the Instituto de Fisica Teorica UAM/CSIC for the
hospitality and support during several visits, where part of this work
was completed. FP wishes to thank the Lawrence Berkeley National
Laboratory for the hospitality during the development of this work; he
also acknowledges the Spanish MEC 'Salvador de Madariaga' programme,
Ref. PRX14/00444. HGM is grateful for support from the UK Science and
Technology Facilities Council through the grant ST/I001204/1. HG
acknowledges the support of the 100 Talents Program of the Chinese
Academy of Sciences. GY wishes to thank MINECO (Spain) for financial
support under project grants AYA2012-31101 and FPA2012-34694. He also
thanks the Red Espanola de Supercomputacion for granting computing time
in the Marenostrum supercomputer, in which part of this work has been
done. AGS, SSA, and JNG acknowledge support from the Transregional
Collaborative Research Centre TR33 'The Dark Universe' of the German
Research Foundation (DFG). AJC is supported by supported by the European
Research Council under the European Community's Seventh Framework
Programme FP7-IDEAS-Phys.LSS 240117. Funding for this work was partially
provided by the Spanish MINECO under project MDM-2014-0369 of ICCUB
(Unidad de Excelencia 'Maria de Maeztu').; The BigMultiDark simulations
have been performed on the SuperMUC supercomputer at the
Leibniz-Rechenzentrum (LRZ) in Munich, using the computing resources
awarded to the PRACE project number 2012060963. We want to thank V.
Springel for providing us with the optimized version of GADGET-2.;
Numerical computations for the power spectrum multipoles and bispectrum
were performed on the Sciama High Performance Compute (HPC) cluster
which is supported by the ICG, SEPNet, and the University of
Portsmouth.; This research also used resources of the National Energy
Research Scientific Computing Center, a DOE Office of Science User
Facility supported by the Office of Science of the US Department of
Energy under Contract No. DE-AC02-05CH11231.; Funding for SDSS-III has
been provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, and the US Department of
Energy Office of Science. The SDSS-III website is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, University of
Cambridge, Carnegie Mellon University, University of Florida, the French
Participation Group, the German Participation Group, Harvard University,
the Instituto de Astrofisica de Canarias, the Michigan State/Notre
Dame/JINA Participation Group, Johns Hopkins University, Lawrence
Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max
Planck Institute for Extraterrestrial Physics, New Mexico State
University, New York University, Ohio State University, Pennsylvania
State University, University of Portsmouth, Princeton University, the
Spanish Participation Group, University of Tokyo, University of Utah,
Vanderbilt University, University of Virginia, University of Washington,
and Yale University.
NR 146
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 4156
EP 4173
DI 10.1093/mnras/stv2826
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800058
ER
PT J
AU McDonald, I
Zijlstra, AA
Sloan, GC
Lagadec, E
Johnson, CI
Uttenthaler, S
Jones, OC
Smith, CL
AF McDonald, I.
Zijlstra, A. A.
Sloan, G. C.
Lagadec, E.
Johnson, C. I.
Uttenthaler, S.
Jones, O. C.
Smith, C. L.
TI EU Del: exploring the onset of pulsation-driven winds in giant stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: AGB and post-AGB; circumstellar matter; stars: individual: EU
Del; stars: mass-loss; stars: winds, outflows
ID INFRARED CLASSIFICATION SPECTROSCOPY; GALACTIC GLOBULAR-CLUSTERS;
FUNDAMENTAL MK STANDARDS; PERIOD VARIABLE-STARS; BRANCH MASS-LOSS;
ALL-SKY SURVEY; DUST PRODUCTION; AGB STARS; RED GIANTS; EVOLVED STARS
AB We explore the wind-driving mechanism of giant stars through the nearby (117 pc), intermediate-luminosity (L approximate to 1600 L-circle dot) star EU Del (HIP 101810, HD 196610). Atacama Pathfinder Experiment observations of the CO (3-2) and (2-1) transitions are used to derive a wind velocity of 9.51 +/- 0.02 km s(-1), a C-12/C-13 ratio of 14(-4)(+9) and a mass-loss rate of a few x 10(-8) M-circle dot yr(-1). Analysis of published spectra show the star has a metallicity of [Fe/H] = -0.27 +/- similar to 0.30 dex. The star's dusty envelope lacks a clear 10-mu m silicate feature, despite the star's oxygen-rich nature. Radiative transfer modelling cannot fit a wind acceleration model which relies solely on radiation pressure on condensing dust. We compare our results to VY Leo (HIP 53449), a star with similar temperature and luminosity, but different pulsation properties. We suggest the much stronger mass-loss from EU Del may be driven by long-period stellar pulsations, due to its potentially lower mass. We explore the implications for the mass-loss rate and wind velocities of other stars.
C1 [McDonald, I.; Zijlstra, A. A.; Jones, O. C.; Smith, C. L.] Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sloan, G. C.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Lagadec, E.] Observ Cote Azur, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA.
[Uttenthaler, S.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Jones, O. C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Smith, C. L.] York Univ, Ctr Res Earth & Space Sci, 4700 Keele St, Toronto, ON M3J 1P3, Canada.
RP McDonald, I (reprint author), Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
EM iain.mcdonald-2@manchester.ac.uk
OI Smith, Christina/0000-0002-6219-8353; Jones, Olivia/0000-0003-4870-5547
FU ESO telescopes [092.F-9328, 094.F-9328]; Clay Fellowship
FX This publication is based on data acquired with the Atacama Pathfinder
Experiment (APEX). APEX is a collaboration between the
Max-Planck-Institut fur Radioastronomie, the European Southern
Observatory and the Onsala Space Observatory. Based on observations made
with ESO telescopes under programme IDs 092.F-9328 and 094.F-9328. CIJ
gratefully acknowledges support from the Clay Fellowship, administered
by the Smithsonian Astrophysical Observatory. The authors are extremely
grateful to Sofia Ramstedt, who reduced the data for this project, both
for her work on the data and for her insightful comments during the
preparation of this manuscript.
NR 99
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 4542
EP 4550
DI 10.1093/mnras/stv2942
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800087
ER
PT J
AU Balokovic, M
Paneque, D
Madejski, G
Furniss, A
Chiang, J
Ajell, M
Alexander, DM
Barret, D
Blandford, RD
Boggs, SE
Christensen, FE
Craig, WW
Forster, K
Giommi, P
Grefenstette, B
Hailey, C
Harrison, FA
Hornstrup, A
Kitaguchi, T
Koglin, JE
Madsen, KK
Mao, PH
Miyasaka, H
Mori, K
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, V
Stern, D
Tagliaferri, G
Urry, CM
Estergaard, NJW
Zhang, WW
Zoglauer, A
Archambault, S
Archer, A
Barnacka, A
Benbow, W
Bird, R
Buckley, JH
Bugaev, V
Cerruti, M
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Huetten, M
Hakansson, N
Holder, J
Humensky, TB
Johnson, CA
Kaaret, P
Kertzman, M
Khassen, Y
Kieda, D
Krause, M
Krennrich, F
Lang, MJ
Maier, G
McArthur, S
Meagher, K
Moriarty, P
Nelson, T
Nieto, D
Ong, RA
Park, N
Poiil, M
Popkow, A
Pueschel, E
Reynolds, PT
Richards, GT
Roache, E
Santander, M
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Todd, NW
Tucci, JV
Tyler, J
Vincent, S
Weinstein, A
Wilhelm, A
Williams, DA
Zitzer, B
Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Banerjee, B
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Biland, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Carmona, E
Carosi, A
Chatterjee, A
Clavero, R
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Da Vela, P
Dazzi, F
De Angelis, A
De Lotto, B
Wilhelmi, ED
Mendez, CD
Di Pierro, E
Prester, DD
Dorner, D
Doro, M
Einecke, S
Elsaesser, D
Fernandez-Barral, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, JG
Garczarczyk, M
Terrats, DG
Gaug, M
Giammaria, P
Glawion, D
Gouinovic, N
Munoz, AG
Guberman, D
Hahn, A
Hanabata, Y
Hayashida, M
Herrera, J
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kodani, K
Konno, Y
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorenz, E
Majumdar, P
Makariev, M
Mallot, K
Maneva, G
Manganaro, M
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Moretti, E
Nakajima, D
Neustroev, V
Niedzwiecki, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palacio, J
Palatiello, M
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Saito, T
Satalecka, K
Scapin, V
Schultz, C
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Stamerra, A
Steinbring, T
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Torres, DF
Toyama, T
Treves, A
Verguilov, V
Vovk, I
Ward, JE
Will, M
Wu, MH
Zanin, R
Perkins, J
Verrecchia, F
Leto, C
Bottcher, M
Villata, M
Raiteri, CM
Acosta-Pulido, JA
Bachev, R
Berdyugin, A
Blinov, DA
Carnerero, MI
Chen, WP
Chinchilla, P
Damljanovic, G
Eswaraiah, C
Grisinna, TS
Ibryamov, S
Jordan, B
Jorstad, SG
Joshi, M
Kopatskaya, EN
Kurtanidze, OM
Kurtanidze, SO
Larionova, EG
Larionova, LV
Larionov, VM
Latev, G
Lin, HC
Marscher, AP
Mokrushina, AA
Morozova, DA
Nikolashvili, MG
Semkov, E
Smith, PS
Strigachev, A
Troitskaya, YV
Troitsky, IS
Vince, O
Barnes, J
Guver, T
Moody, JW
Sadun, AC
Sun, S
Hovatta, T
Richards, JL
Max-Moerbeck, W
Readhead, ACR
Lahteenmaki, A
Tornikoski, M
Tammi, J
Ramakrishnan, V
Reinthal, R
Angelakis, E
Fuhrmann, L
Myserlis, I
Karamanavis, V
Sievers, A
Ungerechts, H
Zensus, JA
AF Balokovic, M.
Paneque, D.
Madejski, G.
Furniss, A.
Chiang, J.
Ajell, M.
Alexander, D. M.
Barret, D.
Blandford, R. D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Forster, K.
Giommi, P.
Grefenstette, B.
Hailey, C.
Harrison, F. A.
Hornstrup, A.
Kitaguchi, T.
Koglin, J. E.
Madsen, K. K.
Mao, P. H.
Miyasaka, H.
Mori, K.
Perri, M.
Pivovaroff, M. J.
Puccetti, S.
Rana, V.
Stern, D.
Tagliaferri, G.
Urry, C. M.
Estergaard, N. J. W.
Zhang, W. W.
Zoglauer, A.
Archambault, S.
Archer, A.
Barnacka, A.
Benbow, W.
Bird, R.
Buckley, J. H.
Bugaev, V.
Cerruti, M.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Huetten, M.
Hakansson, N.
Holder, J.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krause, M.
Krennrich, F.
Lang, M. J.
Maier, G.
McArthur, S.
Meagher, K.
Moriarty, P.
Nelson, T.
Nieto, D.
Ong, R. A.
Park, N.
Poiil, M.
Popkow, A.
Pueschel, E.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Todd, N. W.
Tucci, J. V.
Tyler, J.
Vincent, S.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Banerjee, B.
Bangale, P.
Barres de Almeida, U.
Barrio, J. A.
Becerra Gonzalez, J.
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carmona, E.
Carosi, A.
Chatterjee, A.
Clavero, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
de Ona Wilhelmi, E.
Delgado Mendez, C.
Di Pierro, E.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Garcia Lopez, J.
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giammaria, P.
Glawion (Eisenacher), D.
Gouinovic, N.
Gonzalez Munoz, A.
Guberman, D.
Hahn, A.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorenz, E.
Majumdar, P.
Makariev, M.
Mallot, K.
Maneva, G.
Manganaro, M.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Moretti, E.
Nakajima, D.
Neustroev, V.
Niedzwiecki, A.
Rosillo, M. Nievas
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palacio, J.
Palatiello, M.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Rhode, W.
Ribo, M.
Rico, J.
Rodriguez Garcia, J.
Saito, T.
Satalecka, K.
Scapin, V.
Schultz, C.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Steinbring, T.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Torres, D. F.
Toyama, T.
Treves, A.
Verguilov, V.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Perkins, J.
Verrecchia, F.
Leto, C.
Boettcher, M.
Villata, M.
Raiteri, C. M.
Acosta-Pulido, J. A.
Bachev, R.
Berdyugin, A.
Blinov, D. A.
Carnerero, M. I.
Chen, W. P.
Chinchilla, P.
Damljanovic, G.
Eswaraiah, C.
Grisinna, T. S.
Ibryamov, S.
Jordan, B.
Jorstad, S. G.
Joshi, M.
Kopatskaya, E. N.
Kurtanidze, O. M.
Kurtanidze, S. O.
Larionova, E. G.
Larionova, L. V.
Larionov, V. M.
Latev, G.
Lin, H. C.
Marscher, A. P.
Mokrushina, A. A.
Morozova, D. A.
Nikolashvili, M. G.
Semkov, E.
Smith, P. S.
Strigachev, A.
Troitskaya, Yu. V.
Troitsky, I. S.
Vince, O.
Barnes, J.
Guever, T.
Moody, J. W.
Sadun, A. C.
Sun, S.
Hovatta, T.
Richards, J. L.
Max-Moerbeck, W.
Readhead, A. C. R.
Lahteenmaki, A.
Tornikoski, M.
Tammi, J.
Ramakrishnan, V.
Reinthal, R.
Angelakis, E.
Fuhrmann, L.
Myserlis, I.
Karamanavis, V.
Sievers, A.
Ungerechts, H.
Zensus, J. A.
CA NuSTAR Team
VERITAS Collaboration
MAGIC Collaboration
TI MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED
HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma
rays: general; radiation mechanisms: nonthermal; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS;
PARTICLE-ACCELERATION; LAC OBJECTS; CORRELATED VARIABILITY; TEV BLAZARS;
ELECTRON ACCELERATION; MAGNETIC RECONNECTION; BACKGROUND-RADIATION
AB We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy. (VHE).-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79. keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep Gamma approximate to 3 power law, with no evidence for an exponential cutoff or additional hard components up to similar to 80. keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.
C1 [Balokovic, M.; Forster, K.; Grefenstette, B.; Harrison, F. A.; Madsen, K. K.; Mao, P. H.; Miyasaka, H.; Rana, V.; Hovatta, T.; Readhead, A. C. R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Paneque, D.; Bangale, P.; Barres de Almeida, U.; Borracci, F.; Colin, P.; Dazzi, F.; Doro, M.; Fruck, C.; Hahn, A.; Hose, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moretti, E.; Noda, K.; Rodriguez Garcia, J.; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Vovk, I.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Madejski, G.; Chiang, J.; Blandford, R. D.; Koglin, J. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Madejski, G.; Chiang, J.; Blandford, R. D.; Koglin, J. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Furniss, A.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Ajell, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, D.] CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Boggs, S. E.; Craig, W. W.; Pivovaroff, M. J.; Zoglauer, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.; Hornstrup, A.; Estergaard, N. J. W.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Giommi, P.; Perri, M.; Puccetti, S.; Verrecchia, F.; Leto, C.] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy.
[Hailey, C.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kitaguchi, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Kitaguchi, T.] Hiroshima Univ, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan.
[Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Perri, M.; Puccetti, S.; Verrecchia, F.; Leto, C.] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tagliaferri, G.] Osservatorio Astronomico Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy.
[Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA.
[Zhang, W. W.; Smith, A. W.; Becerra Gonzalez, J.; Perkins, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Archambault, S.; Griffin, S.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Buckley, J. H.; Bugaev, V.; Todd, N. W.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Benbow, W.; Cerruti, M.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Chen, X.; Hakansson, N.; Poiil, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Huetten, M.; Krause, M.; Maier, G.; Poiil, M.; Telezhinsky, I.; Vincent, S.; Wilhelm, A.; Bernardini, E.; Garczarczyk, M.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Richards, J. L.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Dumm, J.; Fortson, L.; Nelson, T.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Humensky, T. B.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[McArthur, S.; Park, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Santander, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Smith, A. W.; Becerra Gonzalez, J.] Univ Maryland, College Pk, MD 20742 USA.
[Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Ahnen, M. L.; Biland, A.; Hughes, G.; Prandini, E.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, E.; Giammaria, P.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy.
[Babic, A.; Prester, D. Dominis; Gouinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia.
[Babic, A.; Prester, D. Dominis; Gouinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia.
[Banerjee, B.; Chatterjee, A.; Majumdar, P.] Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
[Barres de Almeida, U.] Ctr Brasileiro Pesquisas Fis CBPF MCTI, R Dr Xavier Sigaud 150 Urca, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Rosillo, M. Nievas; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain.
[Becerra Gonzalez, J.; Clavero, R.; Colombo, E.; Garcia Lopez, J.; Herrera, J.; Manganaro, M.; Tescaro, D.; Will, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Becerra Gonzalez, J.; Clavero, R.; Colombo, E.; Garcia Lopez, J.; Herrera, J.; Manganaro, M.; Tescaro, D.; Will, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.] Humboldt Univ, Ist Phys, Newtonstr 15, D-12489 Berlin, Germany.
[Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Gonzalez Munoz, A.; Guberman, D.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Palacio, J.; Rico, J.; Ward, J. E.] IFAE, Campus UAB, E-08193 Bellaterra, Spain.
[Bretz, T.; Dorner, D.; Elsaesser, D.; Glawion (Eisenacher), D.; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Bretz, T.] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland.
[Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
[De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.] Univ Padua, I-35131 Padua, Italy.
[De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[de Ona Wilhelmi, E.; Wu, M. H.] CSIC, Inst Space Sci, IEEC, E-08193 Barcelona, Spain.
[Einecke, S.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Frantzen, K.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, E-08193 Bellaterra, Spain.
[Font, L.; Frantzen, K.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, E-08193 Bellaterra, Spain.
[Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Univ Tokyo, ICRR, Japanese MAGIC Consortium, Tokyo 1138654, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Kyoto Univ, Dept Phys, Kyoto 6068501, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Kyoto Univ, Hakubi Ctr, Kyoto 6068501, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Tokai Univ, Hiratsuka, Kanagawa 25912, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Univ Tokushima, KEK, Tokushima, Japan.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland.
[Lopez-Oramas, A.] CEA Saclay, IRFU, DSM, Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Makariev, M.; Maneva, G.; Temnikov, P.; Verguilov, V.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Persic, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy.
[Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland.
[Torres, D. F.] ICREA, E-08193 Barcelona, Spain.
[Torres, D. F.] CSIC, Inst Space Sci, IEEC, E-08193 Barcelona, Spain.
[Treves, A.] Univ Insubria, I-22100 Como, Italy.
[Treves, A.] INFN Milano Bicocca, I-22100 Como, Italy.
[Boettcher, M.] North West Univ, Ctr Space Res, Private Bag X6001,Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa.
[Villata, M.; Raiteri, C. M.; Carnerero, M. I.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Acosta-Pulido, J. A.; Carnerero, M. I.; Chinchilla, P.] Inst Astrofis Canarias, Tenerife, Spain.
[Acosta-Pulido, J. A.; Carnerero, M. I.; Chinchilla, P.] Univ La Laguna, Dept Astrofis, Tenerife, Spain.
[Bachev, R.; Ibryamov, S.; Semkov, E.; Strigachev, A.] Bulgarian Acad Sci, Inst Astron, 72 Tsarigradsko Shosse Blvd, BU-1784 Sofia, Bulgaria.
[Berdyugin, A.; Reinthal, R.] Tuorla Observ, Dept Phys & Astron, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Blinov, D. A.; Grisinna, T. S.; Jorstad, S. G.; Joshi, M.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Larionov, V. M.; Mokrushina, A. A.; Morozova, D. A.; Troitskaya, Yu. V.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, Univ Skij Pr 28, St Petersburg 198504, Russia.
[Blinov, D. A.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Blinov, D. A.] Univ Crete, Inst Plasma Phys, Iraklion 71003, Greece.
[Blinov, D. A.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece.
[Chen, W. P.; Eswaraiah, C.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Zhongli 32001, Taiwan.
[Damljanovic, G.; Vince, O.] Astron Observ, Volgina 7, Belgrade 11060, Serbia.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland.
[Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.] Abastumani Observ, GA-0301 Abastumani, Rep of Georgia.
[Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Kazan, Russia.
[Kurtanidze, O. M.] Guangzhou Univ, Ctr Astrophys, Guangzhou 510006, Guangdong, Peoples R China.
[Larionov, V. M.; Mokrushina, A. A.] Pulkovo Observ, St Petersburg, Russia.
[Latev, G.] Inst Astron, Sofia, Bulgaria.
[Latev, G.] NAO, Sofia, Bulgaria.
[Smith, P. S.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Barnes, J.] Salt Lake Community Coll, Dept Phys, Salt Lake City, UT 84070 USA.
[Guever, T.] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey.
[Moody, J. W.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA.
[Sun, S.] Fudan Univ, Ctr Field Theory & Particle Phys, Shanghai 200433, Peoples R China.
[Sun, S.] Fudan Univ, Dept Phys, Shanghai 200433, Peoples R China.
[Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.; Tammi, J.; Ramakrishnan, V.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland.
[Max-Moerbeck, W.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 13000, FI-00076 Aalto, Finland.
[Angelakis, E.; Fuhrmann, L.; Myserlis, I.; Karamanavis, V.; Zensus, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Sievers, A.; Ungerechts, H.] Inst Radio Astron Milimetr, Ave Divina Pastora 7,Local 20, Granada 18012, Spain.
RP Balokovic, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.; Paneque, D (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.; Madejski, G; Chiang, J (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.; Madejski, G; Chiang, J (reprint author), Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.; Furniss, A (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
EM mislavb@astro.caltech.edu; dpaneque@mppmu.mpg.de; madejski@stanford.edu;
amy.furniss@gmail.com; jchiang@slac.stanford.edu
RI Ramakrishnan, Venkatessh/C-8628-2017; Puljak, Ivica/D-8917-2017;
Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Larionov,
Valeri/H-1349-2013; Grishina, Tatiana/H-6873-2013; Miranda, Jose
Miguel/F-2913-2013; Blinov, Dmitry/G-9925-2013; Delgado,
Carlos/K-7587-2014; Torres, Diego/O-9422-2016; Barrio, Juan/L-3227-2014;
GAug, Markus/L-2340-2014; Cortina, Juan/C-2783-2017; Lahteenmaki,
Anne/L-5987-2013; Font, Lluis/L-4197-2014; Nieto, Daniel/J-7250-2015;
Poutanen, Juri/H-6651-2016; Contreras Gonzalez, Jose Luis/K-7255-2014;
Manganaro, Marina/B-7657-2011; Boggs, Steven/E-4170-2015; Lopez Moya,
Marcos/L-2304-2014; Temnikov, Petar/L-6999-2016; Maneva,
Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Morozova,
Daria/H-1298-2013; Larionova, Elena/H-7287-2013
OI Karamanavis, Vassilis/0000-0003-3133-2617; Angelakis,
Emmanouil/0000-0001-7327-5441; Urry, Meg/0000-0002-0745-9792; de Ona
Wilhelmi, Emma/0000-0002-5401-0744; Bonnoli,
Giacomo/0000-0003-2464-9077; Prandini, Elisa/0000-0003-4502-9053;
Becerra Gonzalez, Josefa/0000-0002-6729-9022; Ramakrishnan,
Venkatessh/0000-0002-9248-086X; Villata, Massimo/0000-0003-1743-6946;
Pueschel, Elisa/0000-0002-0529-1973; Rana, Vikram/0000-0003-1703-8796;
Krause, Maria/0000-0001-7595-0914; Bird, Ralph/0000-0002-4596-8563;
Troitskiy, Ivan/0000-0002-4218-0148; Jorstad,
Svetlana/0000-0001-9522-5453; Larionov, Valeri/0000-0002-4640-4356;
Grishina, Tatiana/0000-0002-3953-6676; Miranda, Jose
Miguel/0000-0002-1472-9690; Blinov, Dmitry/0000-0003-0611-5784; Delgado,
Carlos/0000-0002-7014-4101; Torres, Diego/0000-0002-1522-9065; Barrio,
Juan/0000-0002-0965-0259; GAug, Markus/0000-0001-8442-7877; Cortina,
Juan/0000-0003-4576-0452; Font, Lluis/0000-0003-2109-5961; Nieto,
Daniel/0000-0003-3343-0755; Poutanen, Juri/0000-0002-0983-0049;
Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Manganaro,
Marina/0000-0003-1530-3031; Boggs, Steven/0000-0001-9567-4224; Lopez
Moya, Marcos/0000-0002-8791-7908; Temnikov, Petar/0000-0002-9559-3384;
Morozova, Daria/0000-0002-9407-7804; Larionova,
Elena/0000-0002-2471-6500
FU International Fulbright Science and Technology Award; NASA Headquarters
under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H];
Department of Energy [DE-AC02-765F00515]; NASA [NNX13AO97G, NNG08FD60C,
NNX12AO90G, NNX14AQ58G]; French Space Agency (CNES); National
Aeronautics and Space Administration; U.S. Department of Energy Office
of Science; U.S. National Science Foundation; Smithsonian Institution;
NSERC in Canada; STFC in the U.K.; German BMBF; MPG; Italian INFN; INAF;
Swiss National Fund SNF; ERDF under the Spanish MINECO; Japanese JSPS;
MEXT; Centro de Excelencia Severo Ochoa [SEV-2012-0234, CPAN
CSD2007-00042]; Spanish Consolider-Ingenio programme [CSD2009-00064];
Academy of Finland [268740, 212656, 210338, 121148]; Croatian Science
Foundation (HrZZ) Project [09/176]; University of Rijeka [13.12.1.3.02];
DFG Collaborative Research Centers [SH3823/C4, SH3876/C3]; Polish MNiSzW
grant [745/N-HESS-MAGIC/2010/0]; Russian RFBR [15-02-00949]; St.
Petersburg University [6.38.335.2015]; South African Research Chairs
Initiative (SARChI) of the Department of Science and Technology;
National Research Foundation of South Africa; Institute of Astronomy and
Rozhen National Astronomical Observatory, Bulgaria Academy of Sciences;
Ministry of Education, Science, and Technological Development of the
Republic of Serbia [176011, 176004, 176021]; Scientific Research Fund of
the Bulgarian Ministry of Education and Sciences [DO 02-137
(BIn-13/09)]; Shota Rustaveli National Science Foundation
[FR/638/6-320/12, 31/77]; Istanbul University [49429, 48285]; Bilim
Akademisi (BAGEP program); TUBITAK [13AT100-431, 13AT100-466,
13AT60-430]; NASA grants [NNX08AW31G, NNX11A043G]; NSF grants
[AST-0808050, AST-1109911]
FX M.B. acknowledges support from the International Fulbright Science and
Technology Award, and from NASA Headquarters under the NASA Earth and
Space Science Fellowship Program, grant NNX14AQ07H. This research was
supported in part by the Department of Energy Contract DE-ACO2-765F00515
to the SLAC National Accelerator Center. G.M. and A.F. acknowledge the
support via NASA grant NNX13AO97G. D.B. acknowledges support from the
French Space Agency (CNES) for financial support.; This work was
supported under NASA Contract No. NNG08FD60C and made use of data from
the NuSTAR mission, a project led by the California Institute of
Technology, managed by the Jet Propulsion Laboratory, and funded by the
National Aeronautics and Space Administration. We thank the NuSTAR
Operations, Software, and Calibration teams for support with the
execution and analysis of these observations. This research has made use
of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by
the ASI Science Data Center (ASDC, Italy) and the California Institute
of Technology (USA).; VERITAS is supported by grants from the U.S.
Department of Energy Office of Science, the U.S. National Science
Foundation, and the Smithsonian Institution, by NSERC in Canada, and by
STFC in the U.K. We acknowledge the excellent work of the technical
support staff at the Fred Lawrence Whipple Observatory and at the
collaborating institutions in the construction and operation of the
instrument. The VERITAS Collaboration is grateful to Trevor Weekes for
his seminal contributions and leadership in the field of VHE gamma-ray
astrophysics, which made this study possible.; The MAGIC Collaboration
would like to thank the Institute de Astrofisica de Canarias for the
excellent working conditions at the Observatorio del Roque de los
Muchachos in La Palma. The financial support of the German BMBF and MPG,
the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under
the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully
acknowledged. This work was also supported by the Centro de Excelencia
Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark
CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme,
by grant 268740 of the Academy of Finland, by the Croatian Science
Foundation (HrZZ) Project 09/176 and the University of Rijeka Project
13.12.1.3.02, by the DFG Collaborative Research Centers SH3823/C4 and
SH3876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; The
St. Petersburg University team acknowledges support from Russian RFBR
grant 15-02-00949 and St. Petersburg University research grant
6.38.335.2015.; The work of M.B. is supported by the South African
Research Chairs Initiative (SARChI) of the Department of Science and
Technology and the National Research Foundation of South Africa. Any
opinion, finding, and conclusion or recommendation expressed in this
material is that of the authors and the NRF does not accept any
liability in this regard.; G.D. and O.V. gratefully acknowledge the
observing grant support from the Institute of Astronomy and Rozhen
National Astronomical Observatory, Bulgaria Academy of Sciences. This
work is a part of the Projects No. 176011 (Dynamics and kinematics of
celestial bodies and systems), No. 176004 (Stellar physics), and No.
176021 (Visible and invisible matter in nearby galaxies: theory and
observations) supported by the Ministry of Education, Science, and
Technological Development of the Republic of Serbia.; This research was
partially supported by the Scientific Research Fund of the Bulgarian
Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09).;
The Abastumani team acknowledges financial support of the project
FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under
contract 31/77.; T.G. acknowledges support from Istanbul University
(Project numbers 49429 and 48285), Bilim Akademisi (BAGEP program), and
TUBITAK (project numbers 13AT100-431, 13AT100-466, and 13AT60-430).; The
Boston University effort was supported in part by NASA grants NNX12AO90G
and NNX14AQ58G.; The OVRO 40 m monitoring program is supported in part
by NASA grants NNX08AW31G and NNX11A043G and NSF grants AST-0808050 and
AST-1109911.; The Metsahovi team acknowledges the support from the
Academy of Finland to our observing projects (numbers 212656, 210338,
121148, and others).
NR 120
TC 9
Z9 9
U1 7
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 156
DI 10.3847/0004-637X/819/2/156
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700068
ER
PT J
AU Busquet, G
Estalella, R
Palau, A
Liu, HB
Zhang, QZ
Girart, JM
de Gregorio-Monsalvo, I
Pillai, T
Anglada, G
Ho, PTP
AF Busquet, Gemma
Estalella, Robert
Palau, Aina
Liu, Hauyu Baobab
Zhang, Qizhou
Miquel Girart, Josep
de Gregorio-Monsalvo, Itziar
Pillai, Thushara
Anglada, Guillem
Ho, Paul T. P.
TI WHAT IS CONTROLLING THE FRAGMENTATION IN THE INFRARED DARK CLOUD
G14.225-0.506?: DIFFERENT LEVELS OF FRAGMENTATION IN TWIN HUBS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (G14.225-0.506); stars: formation
ID STAR-FORMING REGIONS; MASSIVE PROTOSTELLAR CORES; DENSE CORES;
HIERARCHICAL FRAGMENTATION; MOLECULAR CLOUD; GALACTIC PLANE; HI-GAL;
LESS-THAN-OR-SIMILAR-TO-1000 AU; TRIGONOMETRIC PARALLAXES; EMBEDDED
CLUSTERS
AB We present observations of the 1.3 mm continuum emission toward hub-N and hub-S of the infrared dark cloud G14.225-0.506 carried out with the Submillimeter Array, together with observations of the dust emission at 870 and 350 mu m obtained with APEX and CSO telescopes. The large-scale dust emission of both hubs consists of a single peaked clump elongated in the direction of the associated filament. At small scales, the SMA images reveal that both hubs fragment into several dust condensations. The fragmentation level was assessed under the same conditions and we found that hub-N presents 4 fragments while hub-S is more fragmented, with 13 fragments identified. We studied the density structure by means of a simultaneous fit of the radial intensity profile at 870 and 350 mu m and the spectral energy distribution adopting a Plummer-like function to describe the density structure. The parameters inferred from the model are remarkably similar in both hubs, suggesting that density structure could not be responsible for determining the fragmentation level. We estimated several physical parameters, such as the level of turbulence and the magnetic field strength, and we found no significant differences between these hubs. The Jeans analysis indicates that the observed fragmentation is more consistent with thermal Jeans fragmentation compared with a scenario in which turbulent support is included. The lower fragmentation level observed in hub-N could be explained in terms of stronger UV radiation effects from a nearby H II region, evolutionary effects, and/or stronger magnetic fields at small scales, a scenario that should be further investigated.
C1 [Busquet, Gemma; Miquel Girart, Josep] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalunya, Spain.
[Busquet, Gemma; Anglada, Guillem] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain.
[Busquet, Gemma; Estalella, Robert] Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, Marti & Franques 1, E-08028 Barcelona, Catalunya, Spain.
[Palau, Aina] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, POB 3-72, Morelia 58090, Michoacan, Mexico.
[Liu, Hauyu Baobab; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Liu, Hauyu Baobab; de Gregorio-Monsalvo, Itziar] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Zhang, Qizhou; Miquel Girart, Josep; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[de Gregorio-Monsalvo, Itziar] JAO, Alonso Cordova 3107, Vitacura, Santiago De Chi, Chile.
[Pillai, Thushara] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RP Busquet, G (reprint author), CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalunya, Spain.; Busquet, G (reprint author), CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain.; Busquet, G (reprint author), Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, Marti & Franques 1, E-08028 Barcelona, Catalunya, Spain.
EM busquet@ice.cat
OI Zhang, Qizhou/0000-0003-2384-6589; Girart, Josep
Miquel/0000-0002-3829-5591
FU Spanish Ministerio de Economia y Competitividad (MINECO)
[FPDI-2013-18204]; Spanish MICINN - FEDER funds [AYA2011-30228-C03,
AYA2014-57369-C3]; UNAM-DGAPA-PAPIIT, Mexico [IA102815]; Deutsche
Forschungsgemeinschaft, DFG via the SPP (priority program) 1573
("Physics of the ISM")
FX The authors are grateful to the anonymous referee for providing comments
that improved the clarity and quality of the paper. G.B. is grateful to
Sergio Molinari and Davide Elia, from the Hi-GAL project, for providing
the Herschel Hi-GAL fluxes to build the SEDs. G.B. acknowledges the
support of the Spanish Ministerio de Economia y Competitividad (MINECO)
under the grant FPDI-2013-18204. G.B., R.E., J.M.G., and G.A. are
supported by the Spanish MICINN grants AYA2011-30228-C03 and
AYA2014-57369-C3 (co-funded with FEDER funds). A.P. acknowledges
financial support from the UNAM-DGAPA-PAPIIT IA102815 grant, Mexico.
T.P. acknowledges financial support from the Deutsche
Forschungsgemeinschaft, DFG via the SPP (priority program) 1573
("Physics of the ISM").
NR 65
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 139
DI 10.3847/0004-637X/819/2/139
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700051
ER
PT J
AU Ching, TC
Lai, SP
Zhang, QZ
Yang, L
Girart, JM
Rao, R
AF Ching, Tao-Chung
Lai, Shih-Ping
Zhang, Qizhou
Yang, Louis
Girart, Josep M.
Rao, Ramprasad
TI HELICAL MAGNETIC FIELDS IN THE NGC 1333 IRAS 4A PROTOSTELLAR OUTFLOWS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (NGC 1333 IRAS 4A); ISM: jets and outflows; ISM:
magnetic fields; stars: formation; submillimeter: ISM; techniques:
polarimetric
ID ZEEMAN CIRCULAR-POLARIZATION; STAR-FORMING REGIONS; CLOSE
BINARY-SYSTEMS; MOLECULAR CLOUDS; LINEAR-POLARIZATION; HIGH-RESOLUTION;
RADIOFREQUENCY LINES; RADIO FREQUENCIES; NGC-1333 IRAS-4; SPECTRAL-LINES
AB We present Submillimeter Array polarization observations of the CO J = 3-2 line toward. NGC 1333 IRAS 4A. The CO Stokes I maps at an angular resolution of similar to 1 '' reveal two bipolar outflows from the binary sources of. NGC 1333 IRAS 4A. The kinematic features of the CO emission can be modeled by wind-driven outflows at similar to 20 degrees inclined from the plane of the sky. Close to the protostars the CO polarization, at an angular resolution of similar to 2.'' 3, has a position angle approximately parallel to the magnetic field direction inferred from the dust polarizations. The CO polarization direction appears to vary smoothly from an hourglass field around the core to an arc-like morphology wrapping around the outflow, suggesting a helical structure of magnetic fields that inherits the poloidal fields at the launching point and consists of toroidal fields at a farther distance of outflow. The helical magnetic field is consistent with the theoretical expectations for launching and collimating outflows from a magnetized rotating disk. Considering that the CO polarized emission is mainly contributed from the low-velocity and low-resolution data, the helical magnetic field is likely a product of the wind-envelope interaction in the winddriven outflows. The CO data reveal a PA of similar to 30 degrees deflection in the outflows. The variation in the CO polarization angle seems to correlate with the deflections. We speculate that the helical magnetic field contributes to similar to 10 degrees deflection of the outflows by means of Lorentz force.
C1 [Ching, Tao-Chung; Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Ching, Tao-Chung; Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Ching, Tao-Chung; Zhang, Qizhou; Girart, Josep M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Lai, Shih-Ping; Rao, Ramprasad] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Yang, Louis] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Girart, Josep M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalonia, Spain.
RP Ching, TC (reprint author), Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.; Ching, TC (reprint author), Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.; Ching, TC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM tching@cfa.harvard.edu
OI Yang, Louis/0000-0003-4026-218X; Girart, Josep
Miquel/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589
FU Smithsonian Predoctoral Fellowship; university consortium of ALMA-Taiwan
Graduate Fellowship; Ministry of Science and Technology (MoST) of Taiwan
[NSC 98-2112-M-007-007-MY3, NSC 101-2119-M-007-004, MoST
102-2119-M-007-004-MY3, MoST 104-2119-M-007-021]; SI CGPS award Magnetic
Fields and Massive Star Formation; MICINN (Spain) [AYA2014-57369-C3];
MECD (Spain) [PRX15/00435]; Smithsonian Institution; Academia Sinica
FX T.C.C. acknowledges the support of the Smithsonian Predoctoral
Fellowship and the university consortium of ALMA-Taiwan Graduate
Fellowship. T.C.C. and S.P.L. are thankful for the support of the
Ministry of Science and Technology (MoST) of Taiwan through Grants NSC
98-2112-M-007-007-MY3, NSC 101-2119-M-007-004, MoST
102-2119-M-007-004-MY3 and MoST 104-2119-M-007-021. Q.Z. acknowledges
the support of the SI CGPS award Magnetic Fields and Massive Star
Formation. J.M.G. acknowledges the support from the MICINN (Spain)
AYA2014-57369-C3 grant and the MECD (Spain) PRX15/00435 travel grant.
The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700071
ER
PT J
AU Graninger, DM
Wilkins, OH
Oberg, KI
AF Graninger, Dawn M.
Wilkins, Olivia H.
Oeberg, Karin I.
TI CARBON CHAINS AND METHANOL TOWARD EMBEDDED PROTOSTARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: molecules; stars: formation; stars: protostars
ID SPITZER SPECTROSCOPIC SURVEY; COMPLEX ORGANIC-MOLECULES; LOW-MASS
PROTOSTARS; YOUNG STELLAR OBJECTS; STAR-FORMATION; DARK CLOUDS;
CHEMISTRY; ICES; GAS; PHASE
AB Large interstellar organic molecules are potential precursors of prebiotic molecules. Their formation pathways and chemical relationships with one another and simpler molecules are therefore of great interest. In this paper we address the relationships between two classes of large organic molecules, carbon chains and saturated complex organic molecules at the early stages of star formation through observations of C4H and CH3OH. We surveyed these molecules with the IRAM 30 m telescope toward 16 deeply embedded low-mass protostars selected from the Spitzer c2d ice survey. We find that CH3OH and C4H are positively correlated, indicating that these two classes of molecules can coexist during the embedded protostellar stage. The C4H/CH3OH gas abundance ratio tentatively correlates with the CH4/CH3OH ice abundance ratio in the same lines of sight. This relationship supports a scenario where carbon chain formation in protostellar envelopes begins with CH4 ice desorption.
C1 [Graninger, Dawn M.; Wilkins, Olivia H.; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Graninger, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dgraninger@cfa.harvard.edu
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Simons Collaboration on
the Origins of Life Investigator award [321183]; Alfred P. Sloan
Foundation; David and Lucile Packard Foundation
FX This work has benefited from discussions with Ryan Loomis, Viviana
Guzman, Edith Fayolle, and from the helpful comments of the anonymous
referee. This study is based on observations with the IRAM 30 m
Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and
IGN (Spain). MO acknowledges funding from the Simons Collaboration on
the Origins of Life Investigator award #321183, the Alfred P. Sloan
Foundation, and the David and Lucile Packard Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
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SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700052
ER
PT J
AU Lin, YT
Mandelbaum, R
Huang, YH
Huang, HJ
Dalal, N
Diemer, B
Jian, HY
Kravtsov, A
AF Lin, Yen-Ting
Mandelbaum, Rachel
Huang, Yun-Hsin
Huang, Hung-Jin
Dalal, Neal
Diemer, Benedikt
Jian, Hung-Yu
Kravtsov, Andrey
TI ON DETECTING HALO ASSEMBLY BIAS WITH GALAXY POPULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: halos; large-scale structure of universe
ID DIGITAL SKY SURVEY; DARK-MATTER HALOS; DISSIPATIONLESS SIMULATIONS;
OCCUPATION DISTRIBUTION; AGE-DEPENDENCE; MASS FUNCTIONS; GROUP FINDER;
SDSS DR7; MODEL; CALIBRATION
AB The fact that the clustering of dark matter halos depends not only on their mass, but also the formation epoch is a prominent, albeit subtle, feature of the cold dark matter structure formation theory and is known as assembly bias. At low-mass scales (similar to 10(12) h(-1) M-circle dot) early-forming halos are predicted to be more strongly clustered than the late forming ones. In this study, we aim to robustly detect the signature of assembly bias observationally, making use of formation time indicators of central galaxies in low-mass halos as a proxy for the halo formation history. Weak gravitational lensing is employed to ensure our early- and late-forming halo samples have similar masses, and are free of contamination of satellites from more massive halos. For the two formation time indicators used (resolved star formation history and current specific star formation rate), we do not find convincing evidence of assembly bias. For a pair of early- and late-forming galaxy samples with mean mass M-200c approximate to 9 x 10(11) h(-1) M-circle dot, the relative bias is 1.00 +/- 0.12. We attribute the lack of detection to the possibilities that either the current measurements of these indicators are too noisy, or they do not correlate well with the halo formation history. Alternative proxies for the halo formation history that should perform better are suggested for future studies.
C1 [Lin, Yen-Ting; Huang, Hung-Jin; Jian, Hung-Yu] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Mandelbaum, Rachel; Huang, Hung-Jin] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Huang, Yun-Hsin; Diemer, Benedikt; Kravtsov, Andrey] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Huang, Yun-Hsin] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Huang, Hung-Jin; Jian, Hung-Yu] Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan.
[Dalal, Neal] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Dalal, Neal] Univ Tokyo, Kavli IPMU WPI, UTIAS, Kashiwa, Chiba 2778583, Japan.
[Dalal, Neal] Univ KwaZulu Natal, Dept Chem & Phys, Univ Rd, Westville, Kzn, South Africa.
[Diemer, Benedikt] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Lin, YT (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
EM ytl@asiaa.sinica.edu.tw
RI Mandelbaum, Rachel/N-8955-2014;
OI Mandelbaum, Rachel/0000-0003-2271-1527; Diemer,
Benedikt/0000-0001-9568-7287
FU Ministry of Science and Technology [MOST 102-2112-M-001-001-MY3, MOST
104-2112-M-001-047]; Department of Energy Early Career Award Program;
Sloan Fellowship; NASA ATP [NNH12ZDA001N]; Kavli Institute for
Cosmological Physics (KICP) at the University of Chicago [NSF
PHY-0551142, PHY-1125897]; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England
FX Y.T.L. dedicates this work to the loving memory of his mother, Ms.
Chun-Chih Kang. We are grateful to Keiichi Umetsu, David Spergel, Jim
Gunn, Cheng Li, Rita Tojeiro, Zheng Zheng, Frank van den Bosch, Masamune
Oguri, Uros Seljak, Lihwai Lin, Chung-Pei Ma, and Ying Zu for helpful
comments, to Gerard Lemson for help with the Millennium Simulation
database, to Surhud More for providing the data used in Figure 4 in
electronic form, and to Bau-Ching Hsieh for help with parallel
computation. We thank the anonymous referee for a constructive report.
Y.T.L. thanks I.H. for constant encouragement and support. Y.T.L.
acknowledges support from the Ministry of Science and Technology grants
MOST 102-2112-M-001-001-MY3 and MOST 104-2112-M-001-047. R.M. is
supported by the Department of Energy Early Career Award Program and by
a Sloan Fellowship. This work was completed in part using the computing
resources provided by the University of Chicago Research Computing
Center. B.D. and A.K. were supported by the NASA ATP grant NNH12ZDA001N
and by the Kavli Institute for Cosmological Physics (KICP) at the
University of Chicago through grants NSF PHY-0551142 and PHY-1125897.;
Funding for the SDSS and SDSS-II has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, the U.S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England. The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions. The SDSS Web Site is http://www.sdss.org/.
The Millennium Simulation databases used in this paper were constructed
as part of the activities of the German Astrophysical Virtual
Observatory (GAVO).
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000372305700031
ER
PT J
AU Oesch, PA
Brammer, G
van Dokkum, PG
Illingworth, GD
Bouwens, RJ
Labbe, I
Franx, M
Momcheva, I
Ashby, MLN
Fazio, GG
Gonzalez, V
Holden, B
Magee, D
Skelton, RE
Smit, R
Spitler, LR
Trenti, M
Willner, SP
AF Oesch, P. A.
Brammer, G.
van Dokkum, P. G.
Illingworth, G. D.
Bouwens, R. J.
Labbe, I.
Franx, M.
Momcheva, I.
Ashby, M. L. N.
Fazio, G. G.
Gonzalez, V.
Holden, B.
Magee, D.
Skelton, R. E.
Smit, R.
Spitler, L. R.
Trenti, M.
Willner, S. P.
TI A REMARKABLY LUMINOUS GALAXY AT Z=11.1 MEASURED WITH HUBBLE SPACE
TELESCOPE GRISM SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark ages, reionization, first stars; galaxies: evolution; galaxies:
formation; galaxies: high-redshift
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; LY-ALPHA EMISSION;
SIMILAR-TO 7; EXTRAGALACTIC LEGACY SURVEY; LENS-AMPLIFIED SURVEY; DEEP
FIELD; CANDIDATE UDFJ-39546284; COSMIC REIONIZATION; SURVEY DESIGN
AB We present Hubble WFC3/IR slitless grism spectra of a remarkably bright z greater than or similar to 10 galaxy candidate, GN-z11, identified initially from CANDELS/GOODS-N imaging data. A significant spectroscopic continuum break is detected at lambda = 1.47 +/- 0.01 mu m. The new grism data, combined with the photometric data, rule out all plausible lower redshift solutions for this source. The only viable solution is that this continuum break is the Lya break redshifted to z(grism) = 11.09(-0.12)(+0.08), just similar to 400Myr after the Big Bang. This observation extends the current spectroscopic frontier by 150 Myr to well before the Planck (instantaneous) cosmic reionization peak at z similar to 8.8, demonstrating that galaxy build-up was well underway early in the reionization epoch at z. >. 10. GN-z11 is remarkably, and unexpectedly, luminous for a galaxy at such an early time: its UV luminosity is 3x. larger than L-* measured at z similar to 6-8. The Spitzer IRAC detections up to 4.5 mu m of this galaxy are consistent with a stellar mass of similar to 10(9) M-circle dot. This spectroscopic redshift measurement suggests that James Webb Space Telescope (JWST) will be able to similarly and easily confirm such sources at z > 10 and characterize their physical properties through detailed spectroscopy. Furthermore, WFIRST, with its wide-field near-IR imaging, would find large numbers of similar galaxies and contribute greatly to JWST ' s spectroscopy, if it is launched early enough to overlap with JWST.
C1 [Oesch, P. A.; van Dokkum, P. G.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Oesch, P. A.; van Dokkum, P. G.; Momcheva, I.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Brammer, G.; Momcheva, I.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Illingworth, G. D.; Holden, B.; Magee, D.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA.
[Bouwens, R. J.; Labbe, I.; Franx, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Ashby, M. L. N.; Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Gonzalez, V.] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile.
[Gonzalez, V.] CATA, Camino Observ 1515, Santiago, Chile.
[Skelton, R. E.] S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Smit, R.] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
[Spitler, L. R.] Macquarie Univ, Fac Sci, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Spitler, L. R.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Trenti, M.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
RP Oesch, PA (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.; Oesch, PA (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RI Gonzalez, Valentino/I-5279-2016; Skelton, Rosalind/S-1845-2016;
OI Skelton, Rosalind/0000-0001-7393-3336; Oesch,
Pascal/0000-0001-5851-6649; Trenti, Michele/0000-0001-9391-305X
FU NASA [NAS5-26555, HST-GO-13871]
FX We thank the anonymous referee for a helpful report, which greatly
improved this manuscript. The primary data for this work were obtained
with the Hubble Space Telescope operated by AURA, Inc. for NASA under
contract NAS5-26555. Furthermore, this work is based in part on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. This work is supported by NASA grant HST-GO-13871.
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SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700041
ER
PT J
AU Ogrean, GA
van Weeren, RJ
Jones, C
Forman, W
Dawson, WA
Golovich, N
Andrade-Santos, F
Murray, SS
Nulsen, P
Roediger, E
Zitrin, A
Bulbul, E
Kraft, R
Goulding, A
Umetsu, K
Mroczkowski, T
Bonafede, A
Randall, S
Sayers, J
Churazov, E
David, L
Merten, J
Donahue, M
Mason, B
Rosati, P
Vikhlinin, A
Ebeling, H
AF Ogrean, G. A.
van Weeren, R. J.
Jones, C.
Forman, W.
Dawson, W. A.
Golovich, N.
Andrade-Santos, F.
Murray, S. S.
Nulsen, P.
Roediger, E.
Zitrin, A.
Bulbul, E.
Kraft, R.
Goulding, A.
Umetsu, K.
Mroczkowski, T.
Bonafede, A.
Randall, S.
Sayers, J.
Churazov, E.
David, L.
Merten, J.
Donahue, M.
Mason, B.
Rosati, P.
Vikhlinin, A.
Ebeling, H.
TI FRONTIER FIELDS CLUSTERS: DEEP CHANDRA OBSERVATIONS OF THE COMPLEX
MERGER MACS J1149.6+2223
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (MACS
J1149.6+2223); galaxies: clusters: intracluster medium
ID MASSIVE GALAXY CLUSTERS; X-RAY SPECTROSCOPY; COLD FRONTS;
PARAMETER-ESTIMATION; TRANSPORT PROCESSES; RADIO-EMISSION; ATOMIC DATA;
ABELL 2146; IMAGES; SAMPLE
AB The Hubble Space Telescope Frontier Fields cluster MACS. J1149.6+2223 is one of the most complex merging clusters, believed to consist of four dark matter halos. We present results from deep (365 ks) Chandra observations of the cluster, which reveal the most distant cold front (z = 0.544) discovered to date. In the cluster outskirts, we also detect hints of a surface brightness edge that could be the bow shock preceding the cold front. The substructure analysis of the cluster identified several components with large relative radial velocities, thus indicating that at least some collisions occur almost along the line of sight. The inclination of the mergers with respect to the plane of the sky poses significant observational challenges at X-ray wavelengths. MACS. J1149.6+2223 possibly hosts a steep-spectrum radio halo. If the steepness of the radio halo is confirmed, then the radio spectrum, combined with the relatively regular ICM morphology, could indicate that MACS. J1149.6+2223 is an old merging cluster.
C1 [Ogrean, G. A.; van Weeren, R. J.; Jones, C.; Forman, W.; Andrade-Santos, F.; Murray, S. S.; Nulsen, P.; Bulbul, E.; Kraft, R.; Randall, S.; David, L.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Dawson, W. A.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA.
[Golovich, N.] Univ Calif Davis, One Shields Ave, Davis, CA 95616 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Nulsen, P.] Univ Western Australia, ICRAR, 35 Stirling Hwy, Crawley, WA 6009, Australia.
[Roediger, E.] Dublin Inst Adv Studies, Astron & Astrophys Sect, 31 Fitzwilliam Pl, Dublin 2, Ireland.
[Roediger, E.] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England.
[Zitrin, A.; Sayers, J.] CALTECH, Cahill Ctr Astron & Astrophys, MC 249-17, Pasadena, CA 91125 USA.
[Goulding, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Mroczkowski, T.] US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Bonafede, A.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Churazov, E.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Churazov, E.] Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Merten, J.] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Mason, B.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Rosati, P.] Univ Ferrara, Dept Phys & Earth Sci, Via G Saragat 1, I-44122 Ferrara, Italy.
[Ebeling, H.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
RP Ogrean, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gogrean@cfa.harvard.edu
RI Churazov, Eugene/A-7783-2013;
OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu,
Keiichi/0000-0002-7196-4822; Nulsen, Paul/0000-0003-0297-4493; van
Weeren, Reinout/0000-0002-0587-1660
FU NASA - Space Telescope Science Institute under NASA
[HST-HF2-51345.001-A, NAS5-26555, HST-HF2-51334.001-A]; NASA - Chandra
X-ray Center [NAS8-03060, PF2-130104]; Clay Fellowship -
Harvard-Smithsonian Center for Astrophysics; National Research Council
Research Associateship Award at the Naval Research Laboratory (NRL);
Chandra grant [G03-14131X]; U.S. DOE by LLNL [DE-AC52-07NA27344]
FX G.A.O. acknowledges support by NASA through a Hubble Fellowship grant
HST-HF2-51345.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555. R.J.v.W. was
supported by NASA through the Einstein Postdoctoral grant number
PF2-130104 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA, under contract
NAS8-03060. R.J.v.W. is supported by a Clay Fellowship awarded by the
Harvard-Smithsonian Center for Astrophysics. A.Z. acknowledges support
by NASA through a Hubble Fellowship grant HST-HF2-51334.001-A awarded by
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. This research was performed while T.M.
held a National Research Council Research Associateship Award at the
Naval Research Laboratory (NRL). F.A.S. acknowledges support from
Chandra grant G03-14131X. Part of this work was performed under the
auspices of the U.S. DOE by LLNL under contract DE-AC52-07NA27344.
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SC Astronomy & Astrophysics
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UT WOS:000372305700025
ER
PT J
AU Street, RA
Udalski, A
Novati, SC
Hundertmark, MPG
Zhu, W
Gould, A
Yee, J
Tsapras, Y
Bennett, DP
Jorgensen, UG
Dominik, M
Andersen, MI
Bachelet, E
Bozza, V
Bramich, DM
Burgdorf, MJ
Cassan, A
Ciceri, S
D'Ago, G
Dong, SB
Evans, DF
Gu, SH
Harkonnen, H
Hinse, TC
Horne, K
Jaimes, RF
Kains, N
Kerins, E
Korhonen, H
Kuffmeier, M
Mancini, L
Menzies, J
Mao, S
Peixinho, N
Popovas, A
Rabus, M
Rahvar, S
Ranc, C
Rasmussen, RT
Scarpetta, G
Schmidt, R
Skottfelt, J
Snodgrass, C
Southworth, J
Steele, IA
Surdej, J
Unda-Sanzana, E
Verma, P
von Essen, C
Wambsganss, J
Wang, YB
Wertz, O
Poleski, R
Pawlak, M
Szymanski, MK
Skowron, J
Mroz, P
Kozlowski, S
Wyrzykowski, L
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
Beichman, C
Bryden, G
Carey, S
Gaudi, BS
Henderson, CB
Pogge, RW
Shvartzvald, Y
Abe, F
Asakura, Y
Bhattacharya, A
Bond, IA
Donachie, M
Freeman, M
Fukui, A
Hirao, Y
Inayama, K
Itow, Y
Koshimoto, N
Li, MCA
Ling, CH
Masuda, K
Matsubara, Y
Muraki, Y
Nagakane, M
Nishioka, T
Ohnishi, K
Oyokawa, H
Rattenbury, N
Saito, T
Sharan, A
Sullivan, DJ
Sumi, T
Suzuki, D
Tristram, J
Wakiyama, Y
Yonehara, A
Han, C
Choi, JY
Park, H
Jung, YK
Shin, IG
AF Street, R. A.
Udalski, A.
Novati, S. Calchi
Hundertmark, M. P. G.
Zhu, W.
Gould, A.
Yee, J.
Tsapras, Y.
Bennett, D. P.
Jorgensen, U. G.
Dominik, M.
Andersen, M. I.
Bachelet, E.
Bozza, V.
Bramich, D. M.
Burgdorf, M. J.
Cassan, A.
Ciceri, S.
D'Ago, G.
Dong, Subo
Evans, D. F.
Gu, Sheng-Hong
Harkonnen, H.
Hinse, T. C.
Horne, Keith
Jaimes, R. Figuera
Kains, N.
Kerins, E.
Korhonen, H.
Kuffmeier, M.
Mancini, L.
Menzies, J.
Mao, S.
Peixinho, N.
Popovas, A.
Rabus, M.
Rahvar, S.
Ranc, C.
Rasmussen, R. Tronsgaard
Scarpetta, G.
Schmidt, R.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Steele, I. A.
Surdej, J.
Unda-Sanzana, E.
Verma, P.
Von Essen, C.
Wambsganss, J.
Wang, Yi-Bo
Wertz, O.
Poleski, R.
Pawlak, M.
Szymanski, M. K.
Skowron, J.
Mroz, P.
Kozlowski, S.
Wyrzykowski, L.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
Beichman, C.
Bryden, G.
Carey, S.
Gaudi, B. S.
Henderson, C. B.
Pogge, R. W.
Shvartzvald, Y.
Abe, F.
Asakura, Y.
Bhattacharya, A.
Bond, I. A.
Donachie, M.
Freeman, M.
Fukui, A.
Hirao, Y.
Inayama, K.
Itow, Y.
Koshimoto, N.
Li, M. C. A.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagakane, M.
Nishioka, T.
Ohnishi, K.
Oyokawa, H.
Rattenbury, N.
Saito, To
Sharan, A.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Tristram, J.
Wakiyama, Y.
Yonehara, A.
Han, C.
Choi, J-Y.
Park, H.
Jung, Y. K.
Shin, I-G.
CA RoboNet Project
MiNDSTEp Consortium
OGLE Project
Spitzer Team
MOA Collaboration
KMTNet Modeling Team
TI SPITZER PARALLAX OF OGLE-2015-BLG-0966: A COLD NEPTUNE IN THE GALACTIC
DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro
ID GRAVITATIONAL LENSING EXPERIMENT; MAGNIFICATION MICROLENSING EVENTS;
DIFFERENCE IMAGE-ANALYSIS; SATELLITE MASS; OGLE-III; PLANETS;
PHOTOMETRY; STARS; BULGE; TELESCOPE
AB We report the detection of a cold Neptune m(planet) = 21 +/- 2M(circle plus) orbiting a 0.38M(circle dot) M dwarf lying 2.5-3.3 kpc toward the Galactic center as part of a campaign combining ground-based and Spitzer observations to measure the Galactic distribution of planets. This is the first time that the complex real-time protocols described by Yee et al., which aim to maximize planet sensitivity while maintaining sample integrity, have been carried out in practice. Multiple survey and follow. up teams successfully combined their efforts within the framework of these protocols to detect this planet. This is the second planet in the Spitzer Galactic distribution sample. Both are in the near. to. mid-disk and are clearly not in the Galactic bulge.
C1 [Street, R. A.; Bachelet, E.] LCOGT, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Udalski, A.; Poleski, R.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Novati, S. Calchi; Beichman, C.] CALTECH, NASA Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
[Novati, S. Calchi; Bozza, V.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2 132, I-84084 Fisciano, Italy.
[Novati, S. Calchi; D'Ago, G.; Scarpetta, G.; Verma, P.] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy.
[Hundertmark, M. P. G.; Jorgensen, U. G.; Harkonnen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M. P. G.; Jorgensen, U. G.; Harkonnen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Gould, A.; Poleski, R.; Gaudi, B. S.; Henderson, C. B.; Pogge, R. W.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Yee, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Tsapras, Y.; Schmidt, R.; Wambsganss, J.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Bennett, D. P.; Bhattacharya, A.; Wakiyama, Y.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Dominik, M.; Horne, Keith; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Juliane Mariesvej 30, DK-2100 Copenhagen O, Denmark.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Dark Cosmol Ctr, Juliane Mariesvej 30, DK-2100 Copenhagen O, Denmark.
[Bachelet, E.; Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, POB 5825, Doha, Qatar.
[Bozza, V.] Inst Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Burgdorf, M. J.] Univ Hamburg, Meteorol Inst, Bundesstr 55, D-20146 Hamburg, Germany.
[Cassan, A.; Ranc, C.] Univ Paris 06, Sorbonne Univ, 98 Bis bd Arago, F-75014 Paris, France.
[Cassan, A.; Ranc, C.] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis bd Arago, F-75014 Paris, France.
[Ciceri, S.; Mancini, L.; Rabus, M.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China.
[Evans, D. F.; Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Gu, Sheng-Hong; Wang, Yi-Bo] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
[Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedukdae Ro, Daejeon 305348, South Korea.
[Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Kains, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Korhonen, H.] ESO FINCA, Finnish Ctr Astron, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Menzies, J.] S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Peixinho, N.; Unda-Sanzana, E.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astron, Avda U Antofagasta, Antofagasta 02800, Chile.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Rasmussen, R. Tronsgaard; Von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, Allee 6 Aout 17,Bat B5c, B-4000 Liege, Belgium.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Bryden, G.; Henderson, C. B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Carey, S.] CALTECH, Spitzer, Ctr Sci, MS 220-6, Pasadena, CA 91109 USA.
[Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nishioka, T.; Oyokawa, H.; Suzuki, D.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan.
[Hirao, Y.; Koshimoto, N.; Nagakane, M.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kyoto 6038555, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand.
[Han, C.; Choi, J-Y.; Park, H.; Jung, Y. K.; Shin, I-G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
RP Street, RA (reprint author), LCOGT, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016; Skowron,
Jan/M-5186-2014; Ranc, Clement/B-1958-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago,
Giuseppe/0000-0001-9697-7331; Skowron, Jan/0000-0002-2335-1730;
Tronsgaard, Rene/0000-0003-1001-0707; Ranc, Clement/0000-0003-2388-4534;
Dominik, Martin/0000-0002-3202-0343; Wang, Yi-Bo/0000-0002-5172-8558
FU National Science Centre, Poland grant MAESTRO [2014/14/A/ST9/00121]; JPL
[1500811]; NSF [AST 1516842, AST-1211875]; NASA; Creative Research
Initiative Program of National Research Foundation of Korea
[2009-0081561]; Regione Campania from POR-FSE Campania; JSPS; NASA
[NNX12AF54G]; NPRP from the Qatar National Research Fund (a member of
Qatar Foundation) [X019-1-006]; Chinese Academy of Sciences
[XDB09000000]; National Natural Science Foundation of China (NSFC)
[11333003, 11390372]; Villum Foundation; Communaut franaise de Belgique
Actions de recherche concertes Acadmie Wallonie-Europe; National Natural
Science Foundation of China [10873031, 11473066]; Gemini-Conicyt Fund
[32120036]; [JSPS23103002]; [JSPS24253004]; [JSPS26247023];
[JSPS25103508]; [23340064]
FX The OGLE project has received funding from the National Science Centre,
Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. Work by J.C.Y., A.G.,
and S.C. was supported by JPL grant 1500811. Work by W.Z. and A.G. was
supported by NSF AST 1516842.r Work by J.C.Y. was performed under
contract with the California Institute of Technology (Caltech)/Jet
Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship
Program executed by the NASA Exoplanet Science Institute. The Spitzer
Team thanks Christopher S. Kochanek for graciously trading us his
allocated observing time on the CTIO 1.3 m during the Spitzer campaign.r
Work by C.H. was supported by the Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea.r G.D.
acknowledges Regione Campania for support from POR-FSE Campania
2014-2020.r T.S. acknowledges the financial support from the JSPS,
JSPS23103002,. JSPS24253004, and JSPS26247023. The MOA project is
supported by the grants JSPS25103508 and 23340064. The US portion of the
MOA Collaboration acknowledges financial support from the NSF
(AST-1211875) and NASA (NNX12AF54G).r Work by Y.S. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA.r This publication was made possible by NPRP grant
#X019-1-006 from the Qatar National Research Fund (a member of Qatar
Foundation).r S.D. is supported by the Strategic Priority Research
Program "The Emergence of Cosmological Structures" of the Chinese
Academy of Sciences (grant No. XDB09000000).r Work by S.M. has been
supported by the Strategic Priority Research Program "The Emergence of
Cosmological Structures" of the Chinese Academy of Sciences Grant No.
XDB09000000, and by the National Natural Science Foundation of China
(NSFC) under grant numbers 11333003 and 11390372.r M.P.G.H. acknowledges
support from the Villum Foundation. Based on data collected by MiNDSTEp
with the Danish 1.54 m telescope at the ESO La Silla observatory. J..
Surdej and O.W. acknowledge support from the Communaut franaise de
Belgique Actions de recherche concertes Acadmie Wallonie-Europe. S.H.G.
and X.B.W. acknowledge the financial support from National Natural
Science Foundation of China through grants Nos. 10873031 and 11473066.r
N.P. acknowledges funding by the Gemini-Conicyt Fund, allocated to the
project No. 32120036.
NR 51
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 93
DI 10.3847/0004-637X/819/2/93
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700005
ER
PT J
AU Watanabe, Y
Sakai, N
Sorai, K
Ueda, J
Yamamoto, S
AF Watanabe, Yoshimasa
Sakai, Nami
Sorai, Kazuo
Ueda, Junko
Yamamoto, Satoshi
TI MOLECULAR DISTRIBUTION IN THE SPIRAL ARM OF M51
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; galaxies: individual (M51); galaxies: ISM; galaxies:
spiral
ID SPECTRAL-LINE SURVEY; SPATIALLY-RESOLVED CHEMISTRY; INTERSTELLAR-MEDIUM;
NEARBY GALAXIES; STAR-FORMATION; NGC 1068; ALMA OBSERVATIONS; 3 MM; GAS;
SHOCKS
AB Molecular line images of (CO)-C-13, (CO)-O-18, CN, CS, CH3OH, and HNCO are obtained toward the spiral arm of M51 at a 7 '' x 6 '' resolution with the Combined Array for Research in Millimeter-wave Astronomy. Distributions of the molecules averaged over a 300 pc scale are found to be almost similar to one another and to essentially trace the spiral arm. However, the principal component analysis shows a slight difference of distributions among molecular species, particularly for CH3OH and HNCO. These two species do not correlate well with the star formation rate, implying that they are not enhanced by local star formation activities but by galactic-scale phenomena such as spiral shocks. Furthermore, the distributions of HNCO and CH3OH are found to be slightly different, and their origins deserve further investigation. The present results provide us with an important clue for. understanding the 300 pc scale chemical composition in the spiral arm and its relation to galactic-scale dynamics.
C1 [Watanabe, Yoshimasa; Sakai, Nami; Yamamoto, Satoshi] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Sakai, Nami] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
[Sorai, Kazuo] Hokkaido Univ, Dept Cosmosci, Dept Phys, Kita Ku, Kita 10,Nishi 8, Sapporo, Hokkaido 0600810, Japan.
[Ueda, Junko] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Ueda, Junko] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Watanabe, Y (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM nabe@taurus.phys.s.u-tokyo.ac.jp
RI Sakai, Nami/N-7438-2015;
OI Sakai, Nami/0000-0002-3297-4497; Watanabe, Yoshimasa/0000-0002-9668-3592
FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris
Foundation; James S. McDonnell Foundation; Associates of the California
Institute of Technology; University of Chicago; state of California;
state of Illinois; state of Maryland; Ministry of Education, Culture,
Sports, Science, and Technology of Japan [21224002, 21740132, 25108005]
FX The authors thank Susanne Aalto for invaluable discussions. The authors
are grateful to the CARMA staff for their excellent support. Support for
CARMA construction was derived from the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S.
McDonnell Foundation, the Associates of the California Institute of
Technology, the University of Chicago, the states of California,
Illinois, and Maryland, and the National Science Foundation. CARMA
development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities. This study is supported by a Grant-in-Aid from the
Ministry of Education, Culture, Sports, Science, and Technology of Japan
(No. 21224002, 21740132, and 25108005).
NR 58
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 144
DI 10.3847/0004-637X/819/2/144
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700056
ER
PT J
AU Baeza, JA
AF Baeza, J. Antonio
TI Molecular phylogeny of porcelain crabs (Porcellanidae: Petrolisthes and
allies) from the south eastern Pacific: the genera Allopetrolisthes and
Liopetrolisthes are not natural entities
SO PEERJ
LA English
DT Article
DE Petrolisthes; Allopetrolisthes; Phylogeny; Liopetrolisthes; Half-crab;
Chile
ID CRUSTACEA DECAPODA PORCELLANIDAE; FAMILIES CHIROSTYLIDAE; ANOMURA
PORCELLANIDAE; ANNOTATED CHECKLIST; LIFE-HISTORY; EVOLUTION; MODEL;
INFERENCE; SEQUENCE; SHRIMPS
AB Porcelain crabs from the closely related genera Petrolisthes, Liopetrolisthes, and Allopetrolisthes are known for their diversity of lifestyles, habitats, and coloration. The evolutionary relationships among the species belonging to these three genera is not fully resolved. A molecular phylogeny of the group may help to resolve the long-standing taxonomic question about the validity of the genera Allopetrohsthes and Liopetrolisthes. Using both 'total evidence' and single-marker analyses based on a 362-bp alignment of the 16S rRNA mitochondrial DNA and a 328-bp alignment of the Histone 3 nuclear DNA, the phylogenetic relationships among 11 species from Petrolisthes (6 species), Liopetrolisthes (2 species), and Allopetrolisthes (3 species), all native to the south eastern Pacific, were examined. The analyses supported three pairs of sister species: L. mitra + L. patagonicus, P. tuberculatus + P. tuberculosus, and A. angulosus + A. punctatus. No complete segregation of species, according to genera, was evident from tree topologies. Bayesian-factor analyses revealed strong support for the unconstrained tree instead of an alternative tree in which monophyly of the three genera was forced. Thus, the present molecular phylogeny does not support the separation of the species within this complex into the genera Petrohsthes, Liopetrolisthes, and Allopetrolisthes. Taking into account the above and other recent molecular phylogenetic analyses focused on other representatives from the family Porcellanidae, it is tentatively proposed to eliminate the genera Liopetrolisthes and Allopetrohsthes, and to transfer their members to the genus Petrolisthes.
C1 [Baeza, J. Antonio] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
[Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA.
[Baeza, J. Antonio] Univ Catolica Norte, Dept Biol Marina, Coquimbo, Iv Region, Chile.
RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.; Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA.; Baeza, JA (reprint author), Univ Catolica Norte, Dept Biol Marina, Coquimbo, Iv Region, Chile.
EM baeza.antonio@gmail.com
OI Baeza, Juan Antonio/0000-0002-2573-6773
NR 60
TC 0
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U1 4
U2 10
PU PEERJ INC
PI LONDON
PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND
SN 2167-8359
J9 PEERJ
JI PeerJ
PD MAR 10
PY 2016
VL 4
AR e1805
DI 10.7717/peerj.1805
PG 18
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG5TR
UT WOS:000372142200015
PM 26989636
ER
PT J
AU Alexander, KD
Berger, E
Guillochon, J
Zauderer, BA
Williams, PKG
AF Alexander, K. D.
Berger, E.
Guillochon, J.
Zauderer, B. A.
Williams, P. K. G.
TI DISCOVERY OF AN OUTFLOW FROM RADIO OBSERVATIONS OF THE TIDAL DISRUPTION
EVENT ASASSN-14li
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: nuclei;
radiation mechanisms: non-thermal; radio continuum: galaxies;
relativistic processes
ID MASSIVE BLACK-HOLE; GAMMA-RAY BURSTS; STAR; JET; VARIABILITY;
SUPERNOVAE; EMISSION; GALAXIES; BRIGHT; SCINTILLATION
AB We report the discovery of transient radio emission from the nearby optically discovered tidal disruption event (TDE) ASASSN-14li (distance of 90 Mpc), making it the first typical TDE detected in the radio, and unambiguously pointing to the formation of a non-relativistic outflow with a kinetic energy of approximate to(4-10) x 10(47) erg, a velocity of approximate to 12,000-36,000 km s(-1), and a mass of approximate to 3 x 10(-5)-7 x 10(-4) M-circle dot. We show that the outflow was ejected on 2014 August 11-25, in agreement with an independent estimate of the timing of super-Eddington accretion based on the optical, ultraviolet, and X-ray observations, and that the ejected mass corresponds to about 1%-10% of the mass accreted in the super-Eddington phase. The temporal evolution of the radio emission also uncovers the circumnuclear density profile, rho(R) proportional to R-2.5 on a scale of about 0.01 pc, a scale that cannot be probed via direct measurements even in the nearest supermassive black holes. Our discovery of radio emission from the nearest well-studied TDE to date, with a radio luminosity lower than all previous limits, indicates that non-relativistic outflows are ubiquitous in TDEs, and that future, more sensitive, radio surveys will uncover similar events.
C1 [Alexander, K. D.; Berger, E.; Guillochon, J.; Zauderer, B. A.; Williams, P. K. G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Alexander, KD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Guillochon, James/0000-0002-9809-8215
FU NSF; NASA; Einstein grant [PF3-140108]; NSF [AST-1302954]
FX K.D.A., E.B., and P.K.G.W. are supported in part by NSF and NASA grants.
J.G. acknowledges support from Einstein grant PF3-140108. A.Z.
acknowledges support from NSF grant AST-1302954. The VLA is operated by
the National Radio Astronomy Observatory, a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 46
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L25
DI 10.3847/2041-8205/819/2/L25
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300009
ER
PT J
AU D'Abrusco, R
Cantiello, M
Paolillo, M
Pota, V
Napolitano, NR
Limatola, L
Spavone, M
Grado, A
Iodice, E
Capaccioli, M
Peletier, R
Longo, G
Hilker, M
Mieske, S
Grebel, EK
Lisker, T
Wittmann, C
van de Ven, G
Schipani, P
Fabbiano, G
AF D'Abrusco, R.
Cantiello, M.
Paolillo, M.
Pota, V.
Napolitano, N. R.
Limatola, L.
Spavone, M.
Grado, A.
Iodice, E.
Capaccioli, M.
Peletier, R.
Longo, G.
Hilker, M.
Mieske, S.
Grebel, E. K.
Lisker, T.
Wittmann, C.
van de Ven, G.
Schipani, P.
Fabbiano, G.
TI THE EXTENDED SPATIAL DISTRIBUTION OF GLOBULAR CLUSTERS IN THE CORE OF
THE FORNAX CLUSTER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: individual (Fornax); galaxies: evolution; galaxies:
individual (NGC 1399)
ID EARLY-TYPE GALAXIES; X-RAY BINARIES; VIRGO CLUSTER; LUMINOSITY FUNCTION;
LARGE-SCALE; NGC 1399; SYSTEM; I.; KINEMATICS; DYNAMICS
AB We report the discovery of a complex extended density enhancement in the Globular Clusters (GCs) in the central similar to 0.5(degrees)(2) (similar to 0.06 Mpc(2)) of the Fornax cluster, corresponding to similar to 50% of the area within 1 core radius. This overdensity connects the GC system of NGC 1399 to most of those of neighboring galaxies within similar to 0 degrees.6 (similar to 210 kpc) along the W-E direction. The asymmetric density structure suggests that the galaxies in the core of the Fornax cluster experienced a lively history of interactions that have left a clear imprint on the spatial distribution of GCs. The extended central dominant structure is more prominent in the distribution of blue GCs, while red GCs show density enhancements that are more centrally concentrated on the host galaxies. We propose that the relatively small-scale density structures in the red GCs are caused by galaxy-galaxy interactions, while the extensive spatial distribution of blue GCs is due to stripping of GCs from the halos of core massive galaxies by the Fornax gravitational potential. Our investigations are based on density maps of candidate GCs extracted from the multi-band VLT Survey Telescope (VST) survey of Fornax (FDS), identified in a three-dimensional color space and further selected based on their g-band magnitude and morphology.
C1 [D'Abrusco, R.; Paolillo, M.; Capaccioli, M.; Longo, G.] Univ Naples Federico II, CU Monte St Angelo, Via Cinthia, I-80126 Naples, Italy.
[Cantiello, M.] INAF Astron Observ Teramo, Via Maggini, I-64100 Teramo, Italy.
[Pota, V.; Napolitano, N. R.; Limatola, L.; Spavone, M.; Grado, A.; Iodice, E.; Schipani, P.] INAF Astron Observ Capodimonte, Via Moiariello 16, I-80131 Naples, Italy.
[Peletier, R.] Univ Groningen, Kapteyn Astron Inst, POB 72, NL-9700 AB Groningen, Netherlands.
[Hilker, M.; Mieske, S.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Grebel, E. K.; Lisker, T.; Wittmann, C.; van de Ven, G.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Fabbiano, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP D'Abrusco, R (reprint author), Univ Naples Federico II, CU Monte St Angelo, Via Cinthia, I-80126 Naples, Italy.
RI Paolillo, Maurizio/J-1733-2012; D'Abrusco, Raffaele/L-2767-2016;
OI Paolillo, Maurizio/0000-0003-4210-7693; D'Abrusco,
Raffaele/0000-0003-3073-0605; /0000-0002-1891-3794; Schipani,
Pietro/0000-0003-0197-589X
NR 44
TC 6
Z9 6
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L31
DI 10.3847/2041-8205/819/2/L31
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300015
ER
PT J
AU Katsuda, S
Maeda, K
Ohira, Y
Yatsu, Y
Mori, K
Aoki, W
Morihana, K
Raymond, JC
Ghavamian, P
Lee, JJ
Shimoda, J
Yamazaki, R
AF Katsuda, Satoru
Maeda, Keiichi
Ohira, Yutaka
Yatsu, Yoichi
Mori, Koji
Aoki, Wako
Morihana, Kumiko
Raymond, John C.
Ghavamian, Parviz
Lee, Jae-Joon
Shimoda, Jiro
Yamazaki, Ryo
TI SPATIALLY RESOLVED SPECTROSCOPY OF A BALMER-DOMINATED SHOCK IN THE
CYGNUS LOOP: AN EXTREMELY THIN COSMIC-RAY PRECURSOR?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; ISM: individual objects (Cygnus Loop); ISM:
supernova remnants; shock waves
ID TYCHOS SUPERNOVA REMNANT; COLLISIONLESS SHOCKS; TELESCOPE; EMISSION;
NOVA; WAVE; HDS
AB We present high-resolution long-slit spectroscopy of a Balmer-dominated shock in the northeastern limb of the Cygnus Loop with the Subaru high dispersion spectrograph. By setting the slit angle along the shock normal, we investigate variations of the flux and profile of the H alpha line from preshock to postshock regions with a spatial resolution of similar to 4 x 10(15) cm. The Ha line profile can be represented by a narrow (28.9 +/- 0.7 km s(-1)) Gaussian in a diffuse region ahead of the shock, i.e., a photoionization precursor, and narrow (33.1 +/- 0.2 km s(-1)) plus broad (130-230 km s(-1)) Gaussians at the shock itself. We find that the width of the narrow component abruptly increases up to 33.1 +/- 0.2 km s(-1), or 38.8 +/- 0.4 km s(-1) if we eliminate projected emission originating from the photoionization precursor, in an unresolved thin layer (less than or similar to 4 x 10(15) cm at a distance of 540 pc) at the shock. We show that the sudden broadening can be best explained by heating via damping of Alfven waves in a thin cosmic-ray (CR) precursor, although other possibilities are not fully ruled out. The thickness of the CR precursor in the Cygnus Loop (a soft gamma-ray emitter) is an order of magnitude thinner than that in Tycho's Knot g (a hard gamma-ray emitter), which may be caused by the different energy distribution of accelerated particles between the two sources. In this context, systematic studies might reveal a positive correlation between the thickness of the CR precursor and the hardness of the CR energy distribution.
C1 [Katsuda, Satoru] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Maeda, Keiichi] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan.
[Ohira, Yutaka; Shimoda, Jiro; Yamazaki, Ryo] Aoyama Gakuin Univ, Dept Phys & Math, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2525258, Japan.
[Yatsu, Yoichi] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ohokayama, Tokyo 1528551, Japan.
[Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys & Elect Engn, 1-1 Gakuen Kibanadai Nishi, Miyazaki 8892192, Japan.
[Aoki, Wako] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Morihana, Kumiko] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, 407-2 Nichigaichi, Sayo, Hyogo 6795313, Japan.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA.
[Lee, Jae-Joon] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
RP Katsuda, S (reprint author), Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
EM katsuda@astro.isas.jaxa.jp
FU Japan Society for the Promotion of Science KAKENHI [25800119, 26800100,
15K05088]; World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan; [HST-GO-13436]
FX We thank all the members of the Subaru telescope, especially Akito
Tajitsu, for performing our observation. We also thank Masaomi Tanaka
for helping our proposal. This work is supported by the Japan Society
for the Promotion of Science KAKENHI Grant Numbers 25800119 (SK),
26800100 (KM), and 15K05088 (RY). The work by K.M. is partly supported
by World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan. J.C.R.'s work was supported by grant
HST-GO-13436 to the Smithsonian Astrophysical Observatory.
NR 23
TC 2
Z9 2
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L32
DI 10.3847/2041-8205/819/2/L32
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300016
ER
PT J
AU Schmidt, R
Sadeghpour, HR
Demler, E
AF Schmidt, Richard
Sadeghpour, H. R.
Demler, E.
TI Mesoscopic Rydberg Impurity in an Atomic Quantum Gas
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SINGLE-ELECTRON; MOLECULES; ABSORPTION; BLOCKADE
AB Giant impurity excitations are powerful probes for exploring new regimes of far out of equilibrium dynamics in few-and many-body quantum systems, and in situ observations of correlations. Motivated by recent experimental progress in spectroscopic studies of Rydberg excitations in ultracold atoms, we develop a new theoretical approach for describing multiscale dynamics of Rydberg excitations in quantum Bose gases. We find that the crossover from few-to many-body dynamics manifests in a dramatic change in spectral profile from resolved molecular lines to broad Gaussian distributions representing a superpolaronic state in which many atoms bind to the Rydberg impurity. We discuss signatures of this crossover in the temperature and density dependence of the spectra.
C1 [Schmidt, Richard; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
[Schmidt, Richard; Demler, E.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Schmidt, R (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
EM richard.schmidt@cfa.harvard.edu
FU NSF [DMR-1308435]; Smithsonian Astrophysical Observatory; Harvard-MIT
CUA; AFOSR Quantum Simulation MURI; ARO-MURI on Atomtronics
FX R. S. and H. R. S. were supported by the NSF through a grant for the
Institute for Theoretical Atomic, Molecular, and Optical Physics at
Harvard University and the Smithsonian Astrophysical Observatory. E. D.
acknowledges support from Harvard-MIT CUA, NSF Grant No. DMR-1308435,
AFOSR Quantum Simulation MURI, the ARO-MURI on Atomtronics, and support
from Dr. Max Rossler, the Walter Haefner Foundation, the ETH Foundation,
and the Simons Foundation. We are thankful to A. Gaj and T. Pfau for
providing data.
NR 55
TC 11
Z9 11
U1 1
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD MAR 10
PY 2016
VL 116
IS 10
AR 105302
DI 10.1103/PhysRevLett.116.105302
PG 6
WC Physics, Multidisciplinary
SC Physics
GA DF9ZX
UT WOS:000371722500004
PM 27015490
ER
PT J
AU Lin, HW
Loeb, A
AF Lin, Henry W.
Loeb, Abraham
TI Zipf's law from scale-free geometry
SO PHYSICAL REVIEW E
LA English
DT Article
ID CITIES; NETWORKS
AB The spatial distribution of people exhibits clustering across a wide range of scales, from household (similar to 10(-2) km) to continental (similar to 10(4) km) scales. Empirical data indicate simple power-law scalings for the size distribution of cities (known as Zipf's law) and the population density fluctuations as a function of scale. Using techniques from random field theory and statistical physics, we show that these power laws are fundamentally a consequence of the scale-free spatial clustering of human populations and the fact that humans inhabit a two-dimensional surface. In this sense, the symmetries of scale invariance in two spatial dimensions are intimately connected to urban sociology. We test our theory by empirically measuring the power spectrum of population density fluctuations and show that the logarithmic slope alpha = 2.04 +/- 0.09, in excellent agreement with our theoretical prediction alpha = 2. The model enables the analytic computation of many new predictions by importing the mathematical formalism of random fields.
C1 [Lin, Henry W.] Harvard Univ, Cambridge, MA 02138 USA.
[Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
RP Lin, HW (reprint author), Harvard Univ, Cambridge, MA 02138 USA.
OI Lin, Henry/0000-0003-2767-6142
FU NSF [AST-1312034]
FX The authors would like to thank the anonymous referees for useful
discussions. This work was supported in part by NSF Grant No.
AST-1312034.
NR 24
TC 1
Z9 1
U1 1
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0045
EI 2470-0053
J9 PHYS REV E
JI Phys. Rev. E
PD MAR 7
PY 2016
VL 93
IS 3
AR 032306
DI 10.1103/PhysRevE.93.032306
PG 6
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA DG0GZ
UT WOS:000371744600013
PM 27078365
ER
PT J
AU Gager, Y
Tarland, E
Lieckfeldt, D
Menage, M
Botero-Castro, F
Rossiter, SJ
Kraus, RHS
Ludwig, A
Dechmann, DKN
AF Gager, Yann
Tarland, Emilia
Lieckfeldt, Dietmar
Menage, Matthieu
Botero-Castro, Fidel
Rossiter, Stephen J.
Kraus, Robert H. S.
Ludwig, Arne
Dechmann, Dina K. N.
TI The Value of Molecular vs. Morphometric and Acoustic Information for
Species Identification Using Sympatric Molossid Bats
SO PLOS ONE
LA English
DT Article
ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; MICROSATELLITE LOCI;
ECHOLOCATION CALLS; CRYPTIC DIVERSITY; CHIROPTERA MOLOSSIDAE;
INSECTIVOROUS BATS; SEQUENCE ALIGNMENT; MITOCHONDRIAL-DNA; HYBRIDIZATION
AB A fundamental condition for any work with free-ranging animals is correct species identification. However, in case of bats, information on local species assemblies is frequently limited especially in regions with high biodiversity such as the Neotropics. The bat genus Molossus is a typical example of this, with morphologically similar species often occurring in sympatry. We used a multi-method approach based on molecular, morphometric and acoustic information collected from 962 individuals of Molossus bondae, M. coibensis, and M. molossus captured in Panama. We distinguished M. bondae based on size and pelage coloration. We identified two robust species clusters composed of M. molossus and M. coibensis based on 18 microsatellite markers but also on a more stringently determined set of four markers. Phylogenetic reconstructions using the mitochondrial gene co1 (DNA barcode) were used to diagnose these microsatellite clusters as M. molossus and M. coibensis. To differentiate species, morphological information was only reliable when forearm length and body mass were combined in a linear discriminant function (95.9% correctly identified individuals). When looking in more detail at M. molossus and M. coibensis, only four out of 13 wing parameters were informative for species differentiation, with M. coibensis showing lower values for hand wing area and hand wing length and higher values for wing loading. Acoustic recordings after release required categorization of calls into types, yielding only two informative subsets: approach calls and two-toned search calls. Our data emphasizes the importance of combining morphological traits and independent genetic data to inform the best choice and combination of discriminatory information used in the field. Because parameters can vary geographically, the multi-method approach may need to be adjusted to local species assemblies and populations to be entirely informative.
C1 [Gager, Yann; Menage, Matthieu; Kraus, Robert H. S.; Dechmann, Dina K. N.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany.
[Gager, Yann; Menage, Matthieu; Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, Constance, Germany.
[Gager, Yann] Univ Konstanz, Int Max Planck Res Sch Organismal Biol, Constance, Germany.
[Tarland, Emilia] Swedish Univ Agr Sci, Dept Anim Breeding & Genet, Uppsala, Sweden.
[Tarland, Emilia; Lieckfeldt, Dietmar; Ludwig, Arne] Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Genet, Berlin, Germany.
[Botero-Castro, Fidel] Univ Montpellier, Inst Sci Evolut, CNRS, IRD,UMR 5554, F-34059 Montpellier, France.
[Rossiter, Stephen J.] Queen Mary Univ London, Sch Biol & Chem Sci, London, England.
[Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Gager, Y (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany.; Gager, Y (reprint author), Univ Konstanz, Dept Biol, Constance, Germany.; Gager, Y (reprint author), Univ Konstanz, Int Max Planck Res Sch Organismal Biol, Constance, Germany.
EM yann.gager@gmail.com
OI Botero-Castro, Fidel/0000-0002-5062-8272
FU German Research Foundation [DFG-GZ DE 1807/3-1]; International Max
Planck Research School for Organismal Biology
FX This work was funded by the German Research Foundation (DFG-GZ DE
1807/3-1 to DKND, http://www.dfg.de/en/index.jsp) and by the
International Max Planck Research School for Organismal Biology (to YG,
http://www.orn.mpg.de/2453/Short_portrait). The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 95
TC 1
Z9 1
U1 7
U2 19
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 4
PY 2016
VL 11
IS 3
AR e0150780
DI 10.1371/journal.pone.0150780
PG 24
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG0FG
UT WOS:000371739400048
PM 26943355
ER
PT J
AU Carrano, MT
Oreska, MPJ
Lockwood, R
AF Carrano, Matthew T.
Oreska, Matthew P. J.
Lockwood, Rowan
TI VERTEBRATE PALEONTOLOGY OF THE CLOVERLY FORMATION (LOWER CRETACEOUS),
II: PALEOECOLOGY
SO JOURNAL OF VERTEBRATE PALEONTOLOGY
LA English
DT Article
ID JUDITH RIVER FORMATION; DINOSAUR PROVINCIAL PARK; FOSSIL ASSEMBLAGES;
NORTH-AMERICA; MICROFOSSIL SITES; SPECIES TURNOVER; MAMMAL EVOLUTION;
BETA DIVERSITY; TERRESTRIAL; HISTORY
AB Vertebrate microfossil assemblages in terrestrial formations are a promising source of data on the structure of fossil metacommunities. However, the degree to which these deposits capture true, metacommunity-level samples is unknown. Individual deposits may be biased in ways that limit their utility for intra- and inter-formation comparisons. This study describes the composition of ten vertebrate microfossil assemblages collected from the Lower Cretaceous Cloverly Formation in Montana and Wyoming, U.S.A., and evaluates whether the assemblages are sufficiently similar to suggest the presence of a single Cloverly metacommunity, or paleocommunity type.' The assemblages appear to be biased by factors related to the preferential incorporation and preservation of different taxa and skeletal element types, which compound with decreasing locality sample size. Less productive localities lack whole taxonomic groups, especially small, fully terrestrial vertebrates. Only the two vertebrate microfossil bonebeds approach the known formation richness. High individual tooth counts overrepresent particular species, especially the crocodylians. Despite these biases, the multiple assemblages nevertheless yield statistically similar taxon abundance rank orders, suggesting the presence of a single, formation-wide paleo-metacommunity, which bears resemblance to a viable metacommunity. The aggregate assemblage exhibits an Eltonian pyramid' trophic hierarchy for both terrestrial and aquatic taxa. Comparing the multiple assemblages synoptically also reveals possible landscape-scale abundance patterns for particular species. Taken together, microvertebrate assemblages offer insight into regional paleo-metacommunities and provide samples for inter-formational comparisons at this level.SUPPLEMENTAL DATASupplemental materials are available for this article for free at www.tandfonline.com/UJVPCitation for this article: Carrano, M. T., M. P. J. Oreska, and R. Lockwood. 2016. Vertebrate paleontology of the Cloverly Formation (Lower Cretaceous), II: Paleoecology. Journal of Vertebrate Paleontology. DOI: 10.1080/02724634.2015.1071265.
C1 [Carrano, Matthew T.; Oreska, Matthew P. J.] Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA.
[Oreska, Matthew P. J.] Univ Virginia, Dept Environm Sci, Clark Hall,291 McCormick Rd,POB 400123, Charlottesville, VA 22904 USA.
[Lockwood, Rowan] Coll William & Mary, Dept Geol, POB 8795, Williamsburg, VA 23185 USA.
RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA.
EM carranom@si.edu; mpo4zx@virginia.edu; rxlock@wm.edu
RI Carrano, Matthew/C-7601-2011
OI Carrano, Matthew/0000-0003-2129-1612
FU Smithsonian Institution; NMNH Equipment Fund; National Science
Foundation through NSF [EAR-1052673]
FX We thank S. Jabo, P. Kroehler, G. Wesley-Hunt, and all of the
participants of the 2004-2010 field expeditions, during which the
materials used in this study were collected. We also thank C. Manuel, R.
Manuel, and E. Kvale for their invaluable advice, support, and
hospitality during that time. F. Grady picked most of the fossils from
the matrix. This research was supported by the Smithsonian Institution
through a Walcott Grant and two Small Grants, as well as the NMNH
Equipment Fund, and by the National Science Foundation through NSF
EAR-1052673 (to MTC). Much of this project was completed as part of a
senior undergraduate honors thesis in geology at the College of William
and Mary by MPJO. We are especially grateful to the Bureau of Land
Management in Wyoming and Montana for their cooperation and permission
to collect the materials studied herein (under permits PA03-WY-102,
PA05-WY-133, PA07-WY-150, PA07-WY-151, PA07-WY-152, and M 100511 to
MTC). Finally, the article was substantially improved thanks to the
careful and thoughtful reviews provided by R. Rogers, D. Brinkman, and
R. Butler.
NR 53
TC 0
Z9 0
U1 1
U2 3
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0272-4634
EI 1937-2809
J9 J VERTEBR PALEONTOL
JI J. Vertebr. Paleontol.
PD MAR 3
PY 2016
VL 36
IS 2
AR e1071265
DI 10.1080/02724634.2015.1071265
PG 12
WC Paleontology
SC Paleontology
GA DH7EA
UT WOS:000372953300007
ER
PT J
AU Carrano, MT
Choiniere, J
AF Carrano, Matthew T.
Choiniere, Jonah
TI NEW INFORMATION ON THE FOREARM AND MANUS OF CERATOSAURUS NASICORNIS
MARSH, 1884 (DINOSAURIA, THEROPODA), WITH IMPLICATIONS FOR THEROPOD
FORELIMB EVOLUTION
SO JOURNAL OF VERTEBRATE PALEONTOLOGY
LA English
DT Article
ID AVIAN HAND; PATAGONIA; PHYLOGENY; HOMOLOGY; WINGS
AB Here we describe the forearm and manus of the ceratosaurian theropod dinosaur Ceratosaurus nasicornis Marsh, 1884, from the Upper Jurassic Morrison Formation of the western U.S.A. Recently removed from exhibition and reprepared, the holotype offers important new information on the morphology of this taxon that bears on the evolution of the forelimb in nonavian theropod dinosaurs more generally. The ulna and radius show particular similarities to those of Dilophosaurus and Eoabelisaurus but lack features that characterize derived abelisaurids. In the manus, Ceratosaurus bears short first phalanges, like more derived taxa in the clade, but retains metacarpals that are much more similar to those of Dilophosaurus, Berberosaurus, and Eoabelisaurus. Taken together, and incorporated with existing phylogenetic data on other ceratosaurs, these data are consistent with the placement of Ceratosaurus as close to Abelisauroidea but basal to Eoabelisaurus. More importantly, they strongly imply that the extremely reduced manus of Limusaurus is a derived condition that does not reflect the primitive state for Ceratosauria and therefore that Averostra is not the most likely placement for a shift in manus digit identity during theropod evolution. Finally, digit reduction began in ceratosaurs that still possessed most phalanges and unguals, and we infer that grasping would have been retained as a primary, if reduced, function in these forms.Citation for this article: Carrano, M. T., and J. Choiniere. 2016. New information on the forearm and manus of Ceratosaurus nasicornis Marsh, 1884 (Dinosauria, Theropoda), with implications for theropod forelimb evolution. Journal of Vertebrate Paleontology. DOI: 10.1080/02724634.2015.1054497.
C1 [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA.
[Choiniere, Jonah] Univ Witwatersrand, DST NRF Ctr Excellence Palaeosci, WITS, Private Bag 3, ZA-2050 Johannesburg, South Africa.
[Choiniere, Jonah] Univ Witwatersrand, Evolutionary Studies Inst, WITS, Private Bag 3, ZA-2050 Johannesburg, South Africa.
RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA.
EM carranom@si.edu; jonah.choiniere@wits.ac.za
RI Carrano, Matthew/C-7601-2011
OI Carrano, Matthew/0000-0003-2129-1612
NR 36
TC 1
Z9 1
U1 3
U2 9
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0272-4634
EI 1937-2809
J9 J VERTEBR PALEONTOL
JI J. Vertebr. Paleontol.
PD MAR 3
PY 2016
VL 36
IS 2
AR e1054497
DI 10.1080/02724634.2015.1054497
PG 14
WC Paleontology
SC Paleontology
GA DH7EA
UT WOS:000372953300003
ER
PT J
AU Buitink, S
Corstanje, A
Falcke, H
Horandel, JR
Huege, T
Nelles, A
Rachen, JP
Rossetto, L
Schellart, P
Scholten, O
ter Veen, S
Thoudam, S
Trinh, TNG
Anderson, J
Asgekar, A
Avruch, IM
Bell, ME
Bentum, MJ
Bernardi, G
Best, P
Bonafede, A
Breitling, F
Broderick, JW
Brouw, WN
Bruggen, M
Buteher, HR
Carbone, D
Ciardi, B
Conway, JE
de Gasperin, E
de Geus, E
Deller, A
Dettmar, RJ
van Diepen, G
Duscha, S
Eisloffel, J
Engels, D
Enriquez, JE
Fallows, RA
Fender, R
Ferrari, C
Frieswijk, W
Garrett, MA
Griessmeier, JM
Gunst, AW
van Haarlem, MP
Hassall, TE
Heald, G
Hessels, JWT
Hoeft, M
Horneffer, A
Iaeobelli, M
Intema, H
Juette, E
Karastergiou, A
Kondratiev, VI
Kramer, M
Kuniyoshi, M
Kuper, G
van Lecuwen, J
Loose, GM
Maat, P
Nann, G
Markoff, S
McFadden, R
McKay-Bukowski, D
McKean, JP
Mevius, M
Mulcahy, DD
Munk, H
Norden, MJ
Orru, E
Paas, H
Pandey-Pommier, M
Pandey, VN
Pietka, M
Pizzo, R
Polatidis, AG
Reich, W
Rotgering, HJA
Scaife, AMM
Schwarz, DJ
Serylak, M
Sluman, J
Smirnov, O
Stappers, BW
Steinmetz, M
Stewart, A
Swinbank, J
Tagger, M
Tang, Y
Tasse, C
Toribio, MC
Vermeulen, R
Vocks, C
Vogt, C
van Weeren, RJ
Wijers, RAMJ
Wijnholds, SJ
Wise, MW
Wucknitz, O
Yatawatta, S
Zarka, P
Zensuss, JA
AF Buitink, S.
Corstanje, A.
Falcke, H.
Hoerandel, J. R.
Huege, T.
Nelles, A.
Rachen, J. P.
Rossetto, L.
Schellart, P.
Scholten, O.
ter Veen, S.
Thoudam, S.
Trinh, T. N. G.
Anderson, J.
Asgekar, A.
Avruch, I. M.
Bell, M. E.
Bentum, M. J.
Bernardi, G.
Best, P.
Bonafede, A.
Breitling, F.
Broderick, J. W.
Brouw, W. N.
Brueggen, M.
Buteher, H. R.
Carbone, D.
Ciardi, B.
Conway, J. E.
de Gasperin, E.
de Geus, E.
Deller, A.
Dettmar, R. -J.
van Diepen, G.
Duscha, S.
Eisloeffel, J.
Engels, D.
Enriquez, J. E.
Fallows, R. A.
Fender, R.
Ferrari, C.
Frieswijk, W.
Garrett, M. A.
Griessmeier, J. M.
Gunst, A. W.
van Haarlem, M. P.
Hassall, T. E.
Heald, G.
Hessels, J. W. T.
Hoeft, M.
Horneffer, A.
Iaeobelli, M.
Intema, H.
Juette, E.
Karastergiou, A.
Kondratiev, V. I.
Kramer, M.
Kuniyoshi, M.
Kuper, G.
van Lecuwen, J.
Loose, G. M.
Maat, P.
Nann, G.
Markoff, S.
McFadden, R.
McKay-Bukowski, D.
McKean, J. P.
Mevius, M.
Mulcahy, D. D.
Munk, H.
Norden, M. J.
Orru, E.
Paas, H.
Pandey-Pommier, M.
Pandey, V. N.
Pietka, M.
Pizzo, R.
Polatidis, A. G.
Reich, W.
Roetgering, H. J. A.
Scaife, A. M. M.
Schwarz, D. J.
Serylak, M.
Sluman, J.
Smirnov, O.
Stappers, B. W.
Steinmetz, M.
Stewart, A.
Swinbank, J.
Tagger, M.
Tang, Y.
Tasse, C.
Toribio, M. C.
Vermeulen, R.
Vocks, C.
Vogt, C.
van Weeren, R. J.
Wijers, R. A. M. J.
Wijnholds, S. J.
Wise, M. W.
Wucknitz, O.
Yatawatta, S.
Zarka, P.
Zensuss, J. A.
TI A large light-mass component of cosmic rays at 10(17)-10(17.5)
electronvolts from radio observations
SO NATURE
LA English
DT Article
ID EXTENSIVE AIR-SHOWERS; ENERGY-SPECTRUM; EMISSION; LOFAR; ARRAY;
SIMULATIONS; TELESCOPE; PULSES
AB Cosmic rays are the highest-energy particles found in nature. Measurements of the mass composition of cosmic rays with energies of 10(17)-10(18) electronvolts are essential to understanding whether they have galactic or extragalactic sources. It has also been proposed that the astrophysical neutrino signal1 comes from accelerators capable of producing cosmic rays of these energies(2). Cosmic rays initiate air showers-cascades of secondary particles in the atmosphere-and their masses can be inferred from measurements of the atmospheric depth of the shower maximum3 (Xmax; the depth of the air shower when it contains the most particles) or of the composition of shower particles reaching the ground(4). Current measurements(5) have either high uncertainty, or a low duty cycle and a high energy threshold. Radio detection of cosmic rays(6-8) is a rapidly developing technique(9) for determining Xmax (refs 10, 11) with a duty cycle of, in principle, nearly 100 per cent. The radiation is generated by the separation of relativistic electrons and positrons in the geomagnetic field and a negative charge excess in the shower front(6,12). Here we report radio measurements of X-max with a mean uncertainty of 16 grams per square centimetre for air showers initiated by cosmic rays with energies of 1017-1017.5 electronvolts. This high resolution in Xmax enables us to determine the mass spectrum of the cosmic rays: we find a mixed composition, with a light-mass fraction (protons and helium nuclei) of about 80 per cent. Unless, contrary to current expectations, the extragalactic component of cosmic rays contributes substantially to the total flux below 10(17.5) electronvolts, our measurements indicate the existence of an additional galactic component, to account for the light composition that we measured in the 10(17)-10(17.5) electronvolt range.
C1 [Buitink, S.] Vrije Univ Brussel, Inst Astrophys, Pleinlaan 2, B-1050 Brussels, Belgium.
[Buitink, S.; Corstanje, A.; Falcke, H.; Hoerandel, J. R.; Nelles, A.; Rachen, J. P.; Rossetto, L.; Schellart, P.; Thoudam, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Falcke, H.; ter Veen, S.; Asgekar, A.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; Deller, A.; van Diepen, G.; Duscha, S.; Enriquez, J. E.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; van Haarlem, M. P.; Heald, G.; Hessels, J. W. T.; Iaeobelli, M.; Kondratiev, V. I.; Kuper, G.; van Lecuwen, J.; Loose, G. M.; Maat, P.; McFadden, R.; McKean, J. P.; Mevius, M.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Toribio, M. C.; Vermeulen, R.; Vogt, C.; Wijnholds, S. J.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Falcke, H.; Hoerandel, J. R.] Nikhef, Sci Pk Amsterdam, NL-1098 XG Amsterdam, Netherlands.
[Falcke, H.; Horneffer, A.; Kramer, M.; Reich, W.; Wucknitz, O.; Zensuss, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Huege, T.] Karlsruhe Inst Technol, Inst Nucl Phys IKP, Postfach 3640, D-76021 Karlsruhe, Germany.
[Nelles, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Scholten, O.; Trinh, T. N. G.] Univ Groningen, KVI Ctr Adv Radiat Technol, NL-9747 AA Groningen, Netherlands.
[Scholten, O.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Anderson, J.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum GEZ, Dept 1, Geodesy & Remote Sensing, Telegrafenberg A17, D-14473 Potsdam, Germany.
[Asgekar, A.] Shell Technol Ctr, Bangalore 560048, Karnataka, India.
[Avruch, I. M.] SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands.
[Avruch, I. M.; Brouw, W. N.; Heald, G.; McKean, J. P.; Mevius, M.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Bell, M. E.] CSIRO Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia.
[Bell, M. E.] Univ Twente, POB 217, NL-7500 AE Enschede, Netherlands.
[Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bernardi, G.; Smirnov, O.] SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa.
[Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bonafede, A.; Brueggen, M.; de Gasperin, E.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Breitling, F.; Nann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Broderick, J. W.; Hassall, T. E.; Mulcahy, D. D.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Buteher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Carbone, D.; Hessels, J. W. T.; van Lecuwen, J.; Markoff, S.; Swinbank, J.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden.
[de Geus, E.] SmarterVision BV, Oostersingel 5, NL-9401 JX Assen, Netherlands.
[Dettmar, R. -J.; Juette, E.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany.
[Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany.
[Engels, D.] Elamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Fender, R.; Karastergiou, A.; Pietka, M.; Serylak, M.; Stewart, A.] Univ Oxford, Dept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Ferrari, C.] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Garrett, M. A.; Intema, H.; Roetgering, H. J. A.; Toribio, M. C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Griessmeier, J. M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France.
[Griessmeier, J. M.] Univ Orleans, OSUC, Stn Radioastron Nancay, Observ Paris,CNRS,INSU,USR 704, Route Souesmes, F-18330 Nancay, France.
[Intema, H.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA.
[Kondratiev, V. I.] Ctr Astro Space, Lebeclev Phys Inst, Profsoyuznayast 84-32, Moscow 117997, Russia.
[Kramer, M.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Kuniyoshi, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, Sodankyla 99600, Finland.
[McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Harwell Sci & Innovation Campus, Didcot OX11 0QX, Oxon, England.
[Paas, H.] Univ Groningen, CIT, POB 72, NL-9700 AB Groningen, Netherlands.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Ave Charles Andre, F-69561 St Gems Laval, France.
[Schwarz, D. J.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany.
[Smirnov, O.; Tasse, C.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Swinbank, J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France.
[Zarka, P.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France.
RP Buitink, S (reprint author), Vrije Univ Brussel, Inst Astrophys, Pleinlaan 2, B-1050 Brussels, Belgium.; Buitink, S (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM Stijn.Buitink@vub.ac.be
RI Intema, Huib/D-1438-2012; Kondratiev, Vladislav/N-1105-2015; Yatawatta,
Sarod/E-6037-2013
OI Intema, Huib/0000-0002-5880-2730; Kondratiev,
Vladislav/0000-0001-8864-7471; Yatawatta, Sarod/0000-0001-5619-4017
FU Netherlands Organization for Scientific Research (NWO), VENI grant
[639-041-130]; Netherlands Research School for Astronomy (NOVA);
Samenwerkingsverband Noord-Nederland (SNN); Foundation for Fundamental
Research on Matter (FOM); European Research Council under the European
Union [227610, 640130]
FX We acknowledge financial support from the Netherlands Organization for
Scientific Research (NWO), VENI grant 639-041-130, the Netherlands
Research School for Astronomy (NOVA), the Samenwerkingsverband
Noord-Nederland (SNN) and the Foundation for Fundamental Research on
Matter (FOM). We acknowledge funding from the European Research Council
under the European Union's Seventh Framework Programme
(FP/2007-2013)/ERC (grant agreement no. 227610) and under the European
Union's Horizon 2020 research and innovation programme (grant agreement
no. 640130). LOFAR, the Low Frequency Array designed and constructed by
ASTRON, has facilities in several countries that are owned by various
parties (each with their own funding sources) and that are collectively
operated by the International LOFAR Telescope (ILT) foundation under a
joint scientific policy.
NR 39
TC 11
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U1 4
U2 23
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAR 3
PY 2016
VL 531
IS 7592
BP 70
EP +
DI 10.1038/nature16976
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF2YW
UT WOS:000371211900041
PM 26935696
ER
PT J
AU Freitas, S
Vavakou, A
Arakelyan, M
Drovetski, SV
Crnobrnja-isailovic, J
Kidov, AA
Cogalniceanu, D
Corti, C
Lymberakis, P
Harris, DJ
Carretero, MA
AF Freitas, Susana
Vavakou, Anna
Arakelyan, Marine
Drovetski, Sergei V.
Crnobrnja-isailovic, Jelka
Kidov, Artem A.
Cogalniceanu, Dan
Corti, Claudia
Lymberakis, Petros
Harris, D. James
Carretero, Miguel A.
TI Cryptic diversity and unexpected evolutionary patterns in the meadow
lizard, Darevskia praticola (Eversmann, 1834)
SO SYSTEMATICS AND BIODIVERSITY
LA English
DT Article
DE Balkans; Caucasus; historical biogeography; phylogeny; phylogeography;
mtDNA; nDNA; pseudo-gene
ID MITOCHONDRIAL-DNA PHYLOGEOGRAPHY; ICE AGES; SPECIES COMPLEX; REPTILIA
SAURIA; TRITURUS NEWTS; WALL LIZARD; LACERTIDAE; BIOGEOGRAPHY;
POPULATION; SQUAMATA
AB Darevskia praticola differs from the other species of the genus in having a large but disjunct distribution, covering the Balkan and the Caucasus regions. Furthermore, most Darevskia species occupy saxicolous habitats, whereas D. praticola inhabits meadows and forest environments. Here we determine the phylogeographic and phylogenetic relationships of Darevskia praticola sensu lato and evaluate the current, morphology-based taxonomy. We sequenced two mtDNA genes (Cyt-b and ND4) and two nuclear loci (MC1R and RELN) for samples collected across the species range. Because our sequences amplified with the Cyt-b primers appear to represent a nuclear pseudogene we excluded this marker from the final analysis. Our results support monophyly of D. praticola and show its division into three clades. The first divergence, dated to the Late Pliocene, is between the Balkans and the Caucasus. The Caucasus lineage is further subdivided in a western Greater Caucasus and a Transcaucasia clade, likely due to subsequent differentiation during the Pleistocene. Our findings do not support the current taxonomic arrangement within D. praticola. The main geographic divergence likely happened due to a vicariance event associated with Plio-Pleistocene climatic and vegetation oscillations.
C1 [Freitas, Susana; Harris, D. James; Carretero, Miguel A.] Univ Porto, CIBIO Res Ctr Biodivers & Genet Resources, InBIO, Campus Agr Vairao,Rua Padre Armando Quintas 7, P-4485661 Vairao, Vila Do Conde, Portugal.
[Freitas, Susana] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Vavakou, Anna] Univ Bielefeld, Fac Biol, D-33615 Bielefeld, Germany.
[Arakelyan, Marine] Yerevan State Univ, Alek Manoogian 1, Yerevan 0025, Armenia.
[Drovetski, Sergei V.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, 1000 Constitution Ave NW, Washington, DC 20004 USA.
[Crnobrnja-isailovic, Jelka] Univ Nis, Fac Sci & Math, Dept Biol & Ecol, Visegradska 33, Nish 18000, Serbia.
[Crnobrnja-isailovic, Jelka] Univ Belgrade, Inst Biol Res Sinisa Stankovic, Dept Evolutionary Biol, Despota Stefana 142, Belgrade 11000, Serbia.
[Kidov, Artem A.] Russian State Agrarian Univ, Fac Anim Sci, Dept Zool, 49 Timiryazevskaya Str, Moscow 127550, Russia.
[Kidov, Artem A.] KA Timiryazev Moscow Agr Acad, 49 Timiryazevskaya Str, Moscow 127550, Russia.
[Cogalniceanu, Dan] Univ Ovidius Constanta, Fac Nat Sci, Bvd Mamaia 124, Constanta, Romania.
[Corti, Claudia] Univ Florence, Museo Storia Nat, Sez Zool La Specola, Via Romana 17, I-50125 Florence, Italy.
[Lymberakis, Petros] Univ Crete, Nat Hist Museum Crete, Knossos Ave, Herakleio 71409, Crete, Greece.
RP Freitas, S (reprint author), Univ Porto, CIBIO Res Ctr Biodivers & Genet Resources, InBIO, Campus Agr Vairao,Rua Padre Armando Quintas 7, P-4485661 Vairao, Vila Do Conde, Portugal.; Freitas, S (reprint author), Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
EM freitas.sn@gmail.com
RI Cogalniceanu, Dan/B-7065-2011; Drovetski, Sergei/A-6002-2011; Carretero,
Miguel/A-1472-2013
OI Cogalniceanu, Dan/0000-0003-2959-014X; Drovetski,
Sergei/0000-0002-1832-5597; Carretero, Miguel/0000-0002-2335-7198
FU FCT [FCOMP-01-0124-FEDER-007062, PTDC/BIA-BEC/101256/2008]; project
"Biodiversity, Ecology and Global Change"; North Portugal Regional
Operational Program (ON.2 - O Novo Norte), under the National Strategic
Reference Framework (NSRF), through the European Regional Development
Fund (ERDF); Gulbenkian Foundation (Portugal); Ministry of Education,
Science and Technological Development of Republic of Serbia [173025]
FX This research was partially funded by FCOMP-01-0124-FEDER-007062 FCT
through the project PTDC/BIA-BEC/101256/2008, by the project
"Biodiversity, Ecology and Global Change" co-financed by North Portugal
Regional Operational Program 2007/2013 (ON.2 - O Novo Norte), under the
National Strategic Reference Framework (NSRF), through the European
Regional Development Fund (ERDF) and by the project "Preserving Armenian
biodiversity: Joint Portuguese - Armenian programme for training in
modern conservation biology" of Gulbenkian Foundation (Portugal). JCI
was funded by Grant No.173025 "Evolution in heterogeneous environments:
adaptation mechanisms, biomonitoring and biodiversity conservation" of
Ministry of Education, Science and Technological Development of Republic
of Serbia.
NR 73
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U1 2
U2 19
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1477-2000
EI 1478-0933
J9 SYST BIODIVERS
JI Syst. Biodivers.
PD MAR 3
PY 2016
VL 14
IS 2
BP 184
EP 197
DI 10.1080/14772000.2015.1111267
PG 14
WC Biodiversity Conservation; Biology
SC Biodiversity & Conservation; Life Sciences & Biomedicine - Other Topics
GA DD3XD
UT WOS:000369855800005
ER
PT J
AU Loaiza, JR
Aguilar, C
De Leon, LF
McMillan, WO
Miller, MJ
AF Loaiza, Jose R.
Aguilar, Celestino
Fernando De Leon, Luis
Owen McMillan, W.
Miller, Matthew J.
TI Mitochondrial genome organization of the Ochre-bellied Flycatcher,
Mionectes oleagineus
SO MITOCHONDRIAL DNA PART A
LA English
DT Article
DE Control region; gene order; mitogenome; suboscine; Tyrannidae
AB We sequenced and compared the mitogenome organization of two specimens of suboscine tyrant flycatcher Mionectes oleagineus from western and eastern Panama, representing distinct mtDNA clades. These samples show identical gene arrangement and vary in size by less than 5 base pairs. Both depict a non-standard avian gene order with an extra non-coding region (e.g. the remnant CR2), which differs in one base pair between them. Small size differences are also found on the control region and the 16S rRNA. Average uncorrected pairwise divergence among protein-coding genes (PCGs) was 2.8, ranging from 1.9% for COXIII and ND6 to 3.2% for ND2 and ATP6, respectively. These mitogenomes may be useful for understanding the evolutionary dynamics of gene order in bird mitochondrial genomes.
C1 [Loaiza, Jose R.; Aguilar, Celestino; Fernando De Leon, Luis; Miller, Matthew J.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Panama City, Panama.
[Owen McMillan, W.; Miller, Matthew J.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Miller, MJ (reprint author), Smithsonian Trop Res Inst Bird Collect, Apartado Postal 0843-03092, Panama City, Panama.
EM millerma@si.edu
OI Miller, Matthew/0000-0002-2939-0239
FU Smithsonian Institution; Smithsonian Tropical Research Institute Office
of Fellowships
FX The authors report no conflict of interest. The authors alone are
responsible for the content and writing of the article. This work was
funded by the Smithsonian Institution and the Smithsonian Tropical
Research Institute Office of Fellowships. We thank Panama's
Environmental Ministry (ANAM) for continued support of scientific
collecting without which this study would not be possible.
NR 6
TC 1
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U1 0
U2 8
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 2470-1394
EI 2470-1408
J9 MITOCHONDRIAL DNA A
JI Mitochondrial DNA Part A
PD MAR 3
PY 2016
VL 27
IS 2
BP 890
EP 891
DI 10.3109/19401736.2014.919491
PG 2
WC Genetics & Heredity
SC Genetics & Heredity
GA CY5RH
UT WOS:000366464400046
PM 24857375
ER
PT J
AU Aguilar, C
De Leon, LF
Loaiza, JR
McMillan, WO
Miller, MJ
AF Aguilar, Celestino
De Leon, Luis Fernando
Loaiza, Jose R.
McMillan, W. Owen
Miller, Matthew J.
TI Extreme sequence divergence between mitochondrial genomes of two
subspecies of White-breasted Wood-wren (Henicorhina leucosticta,
Cabanis, 1847) from western and central Panama
SO MITOCHONDRIAL DNA PART A
LA English
DT Article
DE Mitogenome; multiple species; Troglodytidae
AB Prior studies of mitochondrial variation in White-breasted Wood-Wrens (Henicorhina leucosticta) have suggested that populations in South American and Mesoamerica might represent multiple species. Here we report the complete mitochondrial genomes from two individuals of H. leucosticta, representing the Panamanian subspecies pittieri and alexandri. The two sequences were 16,721 and 16,726 base pairs in size with both genomes comprised of the usual 22 tRNA genes, 2 rRNA genes, 13 protein-coding genes, and one displacement loop region in the standard avian order. Uncorrected pairwise divergence between mitogenome features was high, with the highest divergence occurring in protein-coding genes (average=8.2%), followed by control region (6.7%). RNA features had lower pairwise divergences (average tRNA=4.3%, average rRNA=2.3%). The protein-coding ATPase 6 gene had a different stop codon between these two specimens. The high level of sequence variation between these subspecies suggests that Mesoamerican H. leucosticta might be comprised of multiple species. We urge a full phylogeographic survey of this widespread Neotropical forest bird.
C1 [Aguilar, Celestino; De Leon, Luis Fernando; Loaiza, Jose R.; Miller, Matthew J.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, Panama City, Panama.
[Aguilar, Celestino] Acharya Nagarjuna Univ, Dept Biotechnol, Guntur, India.
[McMillan, W. Owen; Miller, Matthew J.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Miller, MJ (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama.
EM millerma@si.edu
OI Miller, Matthew/0000-0002-2939-0239
FU Smithsonian Institution; Smithsonian Tropical Research Institute Office
of Fellowships
FX The authors report no conflict of interest. The authors alone are
responsible for the content and writing of the article. This work was
funded by the Smithsonian Institution and the Smithsonian Tropical
Research Institute Office of Fellowships.
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U1 1
U2 14
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 2470-1394
EI 2470-1408
J9 MITOCHONDRIAL DNA A
JI Mitochondrial DNA Part A
PD MAR 3
PY 2016
VL 27
IS 2
BP 956
EP 957
DI 10.3109/19401736.2014.926503
PG 2
WC Genetics & Heredity
SC Genetics & Heredity
GA CY5RH
UT WOS:000366464400074
PM 24938093
ER
PT J
AU Baeza, JA
Simpson, L
Ambrosio, LJ
Gueron, R
Mora, N
AF Antonio Baeza, J.
Simpson, Lunden
Ambrosio, Louis J.
Gueron, Rodrigo
Mora, Nathalia
TI Monogamy in a Hyper-Symbiotic Shrimp
SO PLOS ONE
LA English
DT Article
ID CRAB INACHUS-PHALANGIUM; SOCIAL MONOGAMY; SNAPPING SHRIMP; SEA-ANEMONE;
HOST CHARACTERISTICS; CARIBBEAN SEA; MATING SYSTEM; LIFE-HISTORY;
PINNA-CARNEA; DECAPODA
AB Theory predicts that monogamy is adaptive in resource-specialist symbiotic crustaceans inhabiting relatively small and morphologically simple hosts in tropical environments where predation risk away from hosts is high. We tested this prediction in Pontonia manningi, a hyper-symbiotic shrimp that dwells in the mantle cavity of the Atlantic winged oyster Pteria colymbus that, in turn, infects gorgonians from the genus Pseudopterogorgia in the Caribbean Sea. In agreement with theory, P. manningi were found dwelling as heterosexual pairs in oysters more frequently than expected by chance alone. Males and females also inhabited the same host individual independent of the female gravid condition or of the developmental stage of brooded embryos. While the observations above argue in favor of monogamy in P. manningi, there is evidence to suggest that males of the studied species are moderately promiscuous. That females found living solitary in oysters most often brooded embryos, and that males allocated more to weaponry (major claw size) than females at any given size suggest that males might be roaming among host individuals in search of and, fighting for, receptive females. All available information depicts a rather complex mating system in P. manningi: primarily monogamous but with moderately promiscuous males.
C1 [Antonio Baeza, J.; Simpson, Lunden; Ambrosio, Louis J.] Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA.
[Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
[Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
[Gueron, Rodrigo] Inst Fed Educ Ciencia & Tecnol Espirito Santo, Campus Alegre, Vitoria, ES, Brazil.
[Mora, Nathalia] Univ Valle, Fac Ciencias, Dept Biol, Cali 760032, Colombia.
RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA.; Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.; Baeza, JA (reprint author), Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
EM jbaezam@clemson.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
FU Clemson University
FX This study was funded by start up money from Clemson University to JAB.
NR 52
TC 0
Z9 0
U1 1
U2 1
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 2
PY 2016
VL 11
IS 3
AR e0149797
DI 10.1371/journal.pone.0149797
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG0AN
UT WOS:000371724200053
PM 26934109
ER
PT J
AU Dove, CJ
Wickler, S
AF Dove, Carla J.
Wickler, Stephen
TI Identification of Bird Species Used to Make a Viking Age Feather Pillow
SO ARCTIC
LA English
DT Article
DE northern Norway; Vesteralen islands; Viking Age; boat grave; pillow;
birds; feathers; microstructure
AB A grave containing the remains of a wooden boat was discovered in 1934 under a low mound in a bog at Oksnes in the Vesteralen islands of northern Norway. The boat grave dates to the 10th century in the Viking Age, and grave goods placed in the boat include an iron axe, a cowhide in which the body was wrapped, and pillow remains consisting of feather stuffing and a wool textile cover. A microscopic analysis of the feathers from a subsample of the pillow fill identified three avian orders: Anseriformes (eider); Suliformes (cormorant), and Charadriiformes (unspecified gull). It was possible to make one species-level identification of Great Cormorant (Phalacrocorax carbo) and to narrow the gull types to the "white-headed" gull group. The sample was composed of a nearly equal mix of downy and pennaceous feather types. Downy feathers from gulls (Laridae) composed the majority of the material in this sample. While it is reported that feathers and down (assumed to be eider) were used in the Late Iron Age, this is the first successful attempt to identify bird species used in these materials and suggests that avian species identifications should be explored in other such burial items to enhance our understanding of human-wildlife interactions throughout Norse history.
C1 [Dove, Carla J.] Smithsonian Inst, Div Birds, Feather Identificat Lab, NHB E-600,MRC 116, Washington, DC 20560 USA.
[Wickler, Stephen] Univ Tromso, Tromso Univ Museum, Dept Cultural Sci, N-9037 Tromso, Norway.
RP Dove, CJ (reprint author), Smithsonian Inst, Div Birds, Feather Identificat Lab, NHB E-600,MRC 116, Washington, DC 20560 USA.
EM dovec@si.edu; Stephen.wickler@uit.no
FU U.S. military; Federal Aviation Administration
FX Animal hair was identified at the laboratory of the Department of
Archaeology, University of Helsinki, by Tuija Kirkinen, who kindly gave
us permission to cite her preliminary results. The Feather
Identification Lab, Smithsonian Institution, is funded through
interagency agreements with the U.S. military and the Federal Aviation
Administration. Sally Bensusen illustrated the feather figure. The map
and pillow photos were provided by Adnan Icagic, and the grave photos,
by T. Soot-Ryan. Smithsonian Institution Libraries assisted with
interlibrary loans. All of the molecular laboratory work was conducted
by Faridah Dahlan, with the support of the facilities of the
Laboratories of Analytical Biology, National Museum of Natural History.
Sergei Drovetski translated the Russian abstract. We thank W. Fitzhugh
for comments on an early version of the manuscript.
NR 27
TC 0
Z9 0
U1 1
U2 1
PU ARCTIC INST N AMER
PI CALGARY
PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER,
CALGARY, ALBERTA T2N 1N4, CANADA
SN 0004-0843
EI 1923-1245
J9 ARCTIC
JI Arctic
PD MAR
PY 2016
VL 69
IS 1
BP 29
EP 36
DI 10.14430/arctic4546
PG 8
WC Environmental Sciences; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA DY3LE
UT WOS:000384993100003
ER
PT J
AU Deans, E
AF Deans, Elizabeth
TI Display of Art in the Roman Palace, 1550-1750
SO WEST 86TH-A JOURNAL OF DECORATIVE ARTS DESIGN HISTORY AND MATERIAL
CULTURE
LA English
DT Book Review
C1 [Deans, Elizabeth] George Mason Univ, Smithsonian Inst, Fairfax, VA 22030 USA.
RP Deans, E (reprint author), George Mason Univ, Smithsonian Inst, Fairfax, VA 22030 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 2153-5531
EI 2153-5558
J9 WEST 86TH
JI West 86th
PD SPR-SUM
PY 2016
VL 23
IS 1
BP 137
EP 139
PG 4
WC Art
SC Art
GA DW7VM
UT WOS:000383860900012
ER
PT J
AU Sigala, I
Lozano-Garcia, S
Escobar, J
Perez, L
Gallegos-Neyra, E
AF Sigala, Itzel
Lozano-Garcia, Socorro
Escobar, Jaime
Perez, Liseth
Gallegos-Neyra, Elvia
TI Testate Amoebae (Amebozoa: Arcellinida) in Tropical Lakes of Central
Mexico
SO REVISTA DE BIOLOGIA TROPICAL
LA English
DT Article
DE protozoa; amoeboid; thecamoebians; taxonomy; biometry
ID ARCELLACEANS THECAMOEBIANS; AMOEBOZOA; IDENTIFICATION; CONTAMINATION;
BIOGEOGRAPHY; INDICATORS; DIVERSITY; ONTARIO; CANADA; TOOLS
AB Testate amoebae are common single-celled eukaryotic organisms in aquatic ecosystems. Despite their important role in these ecosystems, and their potential as bioindicators and paleoindicators, they remain poorly studied in Mexico. The major objectives of this study were to: 1) increase knowledge of testate amoebae in Mexico's tropical lakes, and 2) create a catalog of high-quality scanning electron micrographs that can be used for future ecological and paleoenvironmental studies. We collected surface-sediment samples from 29 lakes, located in the Transmexican Volcanic Belt, one at each lake during June and October 2011, and March 2013. Sediments were collected with an Ekman grab and preserved in anhydrous ethanol. Sub-samples were observed under a stereomicroscope and morphometric data for each species were recorded. Total diameter and aperture diameter were measured on circular tests. Irregularly shaped tests were measured for length and width of the aperture and for the size of the whole test. If a specimen possessed spines, the length of one randomly selected spine was measured. The best-preserved specimen of each taxon was photographed with an optical microscope and a scanning electron microscope (SEM). We found 41 taxa of testate amoebae belonging to the genera: Arcella, Argynnia, Centropyxis, Cucurbitella, Cyclopyxis, Cyphoderia, Difflugia, Euglypha, Lesquereusia, Pentagonia, Pseudodifflugia and Scutiglypha. Twelve species not previously reported for Mexico were recorded, along with 13 varieties. The average number of taxa recorded in each lake was eight, and the highest taxonomic richness was 18. The taxon found in the greatest number of lakes was Centropyxis aculeata var. aculeata. Taxonomic richness varied among lakes in the same region. This could reflect lake-specific differences in environmental conditions, underscoring the need for more detailed studies that include collection of data on physical and chemical variables in the lakes. Our results highlighted the need of further studies for the distribution patterns and ecology of lacustrine testate amoebae.
C1 [Sigala, Itzel] Univ Nacl Autonoma Mexico, Inst Geol, Posgrado Ciencias Biol, Ciudad Univ, Mexico City 04510, DF, Mexico.
[Lozano-Garcia, Socorro; Perez, Liseth] Univ Nacl Autonoma Mexico, Inst Geol, Ciudad Univ, Mexico City 04510, DF, Mexico.
[Escobar, Jaime] Univ Norte, Dept Ingn Civil & Ambiental, Km 5 Via Puerto Colombia, Barranquilla, Colombia.
[Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City 0843033092, Panama.
[Gallegos-Neyra, Elvia] Univ Nacl Autonoma Mexico, Fac Estudios Super Iztacala, Lab Invest Patogenos Emergentes, Unidad Invest Interdisciplinaria Ciencias Salud &, Los Reyes Iztacala 54090, Estado De Mexic, Mexico.
RP Sigala, I (reprint author), Univ Nacl Autonoma Mexico, Inst Geol, Posgrado Ciencias Biol, Ciudad Univ, Mexico City 04510, DF, Mexico.
EM itzelsr@yahoo.com.mx; mslozano@unam.mx; jhescobar@uninorte.edu.com;
lcpereza@geologia.unam.mx; elvia.gallegos1@gmail.com
FU CONACYT [167 621]; NSF [0 902 864]; Instituto de Geologia, Universidad
Nacional Autonoma de Mexico
FX We thank the Posgrado de Ciencias Biologicas, UNAM (CVU 294 479
CONACYT). This research was funded by grants from CONACYT (167 621), NSF
(0 902 864) and the Instituto de Geologia, Universidad Nacional Autonoma
de Mexico, for financial support. We thank Margarita Caballero and Edyta
Zawisza (Instituto de Geofisica, UNAM), Alexander Correa-Metrio and
Esperanza Tones (Instituto de Geologia, UNAM) for field help. Special
thanks to Alejandro Angeles, Mariela Esquivel, Jacqueline Jasso, Antonio
Guerra and Manuel Valle for help in laboratory. We thank Natalia Hoyos
for the map elaboration, Enrique Lara and Anatoly Bobrov for help with
identifications of some species and Mark Brenner for editorial
assistance.
NR 45
TC 0
Z9 0
U1 3
U2 3
PU REVISTA DE BIOLOGIA TROPICAL
PI SAN JOSE
PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA
RICA
SN 0034-7744
EI 2215-2075
J9 REV BIOL TROP
JI Rev. Biol. Trop.
PD MAR
PY 2016
VL 64
IS 1
BP 377
EP 397
PG 21
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA DU1FK
UT WOS:000381953400031
ER
PT J
AU Hershler, R
Liu, HP
Stevens, LE
AF Hershler, Robert
Liu, Hsiu-Ping
Stevens, Lawrence E.
TI A NEW SPRINGSNAIL (HYDROBIIDAE: PYRGULOPSIS) FROM THE LOWER COLORADO
RIVER BASIN, NORTHWESTERN ARIZONA
SO WESTERN NORTH AMERICAN NATURALIST
LA English
DT Article
ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; SNAILS;
CAENOGASTROPODA; SYSTEMATICS; CALIFORNIA
AB We describe a new springsnail species, Pyrgulopsis hualapaiensis, from the Lower Colorado River basin (northwestern Arizona) that has an ovate-to narrow-conic shell and narrow penis ornamented with a small gland on the distal edge of the lobe. This new species differs from closely similar congeners from the Lower Colorado River basin in several details of female reproductive anatomy and in its mtCOI haplotype (3.0%-5.0% mean sequence divergence). Bayesian, maximum parsimony, and distance-based phylogenetic analyses of COI data congruently resolved P hualapaiensis as sister to a divergent lineage of Pyrgulopsis thompsoni in the middle Gila River watershed (southeastern Arizona), although this relationship was not well supported. Pyrgulopsis hualapaiensis is endemic to a spring complex in the Hualapai Indian Reservation that is a culturally sensitive site for the tribe. The small population of these snails appears to be robust despite recent habitat modifications (trenching of outflow and construction of a spring box) and disturbance from road traffic. Future conservation measures could include monitoring of the population and augmentation of the gravel habitat used by these snails.
C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Liu, Hsiu-Ping] Metropolitan State Univ, Dept Biol, Denver, CO 80217 USA.
[Stevens, Lawrence E.] Museum Northern Arizona, Flagstaff, AZ 86001 USA.
RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
EM hershlerr@si.edu
NR 30
TC 1
Z9 1
U1 1
U2 1
PU BRIGHAM YOUNG UNIV
PI PROVO
PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA
SN 1527-0904
EI 1944-8341
J9 WEST N AM NATURALIST
JI West. North Am. Naturalist
PD MAR
PY 2016
VL 76
IS 1
BP 72
EP 81
PG 10
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DS6GB
UT WOS:000380879000007
ER
PT J
AU Collins, M
AF Collins, Martin
TI Untitled
SO HISTORY AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Collins, Martin] Smithsonian Inst, Washington, DC 20560 USA.
RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
EM CollinsM@si.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0734-1512
EI 1477-2620
J9 HIST TECHNOL
JI Hist. Technol.
PD MAR
PY 2016
VL 32
IS 1
BP 1
EP 1
DI 10.1080/07341512.2016.1196557
PG 1
WC History
SC History
GA DP5PL
UT WOS:000378549500001
ER
PT J
AU Daly, L
French, K
Miller, TL
Eoin, LN
AF Daly, Lewis
French, Katherine
Miller, Theresa L.
Eoin, Luiseach Nic
TI INTEGRATING ONTOLOGY INTO ETHNOBOTANICAL RESEARCH
SO JOURNAL OF ETHNOBIOLOGY
LA English
DT Article
ID TRADITIONAL ECOLOGICAL KNOWLEDGE; BIODIVERSITY CONSERVATION; NICHE
CONSTRUCTION; MANAGEMENT; PLANTS; LANDSCAPES; AUSTRALIA; CULTURES;
PEOPLE
C1 [Daly, Lewis] Univ Oxford, Inst Social & Cultural Anthropol, 51-53 Banbury Rd, Oxford OX2 6PE, England.
[French, Katherine] Univ Oxford, Dept Plant Sci, Oxford OX2 6PE, England.
[Miller, Theresa L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
[Eoin, Luiseach Nic] Univ Oxford, Inst Archaeol, Oxford OX2 6PE, England.
RP Daly, L (reprint author), Univ Oxford, Inst Social & Cultural Anthropol, 51-53 Banbury Rd, Oxford OX2 6PE, England.
EM lewisjdaly@gmail.com
OI Nic Eoin, Luiseach/0000-0002-2497-1966
NR 72
TC 1
Z9 1
U1 2
U2 2
PU SOC ETHNOBIOLOGY
PI DENTON
PA UNIV NORTH TEXAS, DEPT GEOGRAPHY, 1155 UNION CIRCLE 305279, DENTON, TX
76203-5017 USA
SN 0278-0771
EI 2162-4496
J9 J ETHNOBIOL
JI J. Ethnobiol.
PD MAR
PY 2016
VL 36
IS 1
BP 1
EP 9
PG 9
WC Anthropology; Biology
SC Anthropology; Life Sciences & Biomedicine - Other Topics
GA DO1LP
UT WOS:000377539900001
ER
PT J
AU Miller, TL
AF Miller, Theresa L.
TI LIVING LISTS: HOW THE INDIGENOUS CANELA COME TO KNOW PLANTS THROUGH
ETHNOBOTANICAL CLASSIFICATION
SO JOURNAL OF ETHNOBIOLOGY
LA English
DT Article
DE biodiversity; plants; indigenous Canela; northeast Brazil; childcare
ID BRAZILIAN CERRADO; MANIOC; DOMESTICATION; CREATIVITY; DIVERSITY; SAVANNA
AB This paper explores how members of the indigenous Canela community of northeast Brazil value and make meaningful their engagements with cultivated plants in their local Cerrado ("savannah") environment through the recent creation of written ethnobotanical lists and through more traditional multi-sensory, embodied approaches. It compares the traditional approach of Canela gardeners coming to know and "becoming with" growing plants through caring, affectionate activities such as garden visits, ritual singing, food sharing, and shamanic communication, with that of the recent written documentation of ethnobotanical knowledge that is associated with people and things coming from a world "outside" the community. Through the creation of fluid and dynamic living lists, Canela gardener parents are seeking new and innovative ways to engage with and know the plant children growing in their gardens. Both the traditional and newer approaches to plant knowledge can and do co-exist in the community. Moreover, Canela gardeners are embracing and working through the "ontological frictions" that emerge between disparate ways of knowing about and of becoming alongside cultivated plants. The Canela case can contribute to a broader understanding of biodiversity management as "childcare" and encourage a deeper engagement with both humans' and plants' perspectives in future ethnobotanical studies.
C1 [Miller, Theresa L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 10th & Constitut Ave NW, Washington, DC 20560 USA.
RP Miller, TL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 10th & Constitut Ave NW, Washington, DC 20560 USA.
EM millerth@si.edu
FU University of Oxford's Institute of Social and Cultural Anthropology and
Linacre College; University of Washington-Whatcom Museum; BioSocial
Society
FX Funding for the doctoral fieldwork was provided by the Rausing
Scholarship from the University of Oxford's Institute of Social and
Cultural Anthropology and Linacre College, the Jacobs Research Funds
from the University of Washington-Whatcom Museum, and the BioSocial
Society. Special thanks goes to my doctoral supervisor at the University
of Oxford, Dr. Laura Rival, my Brazilian supervisor Dr. Carlos Fausto
from the Federal University of Rio de Janeiro, and Dr. William Crocker
from the Smithsonian Institution's National Museum of Natural History
for their support throughout the fieldwork and dissertation writing. I
thank Dr. Stephen Harris, Department of Plant Sciences, University of
Oxford, for identifying the species and genera of the pankryt and pat
juhtoi-re categories of beans during a meeting in May 2014. Thanks also
goes to the three anonymous reviewers for their detailed reading and
helpful commentary. Finally, I especially thank the Canela research
assistants and the community at large for their curiosity, creativity,
and enthusiasm for gardening and plant childcare.
NR 58
TC 0
Z9 0
U1 4
U2 4
PU SOC ETHNOBIOLOGY
PI DENTON
PA UNIV NORTH TEXAS, DEPT GEOGRAPHY, 1155 UNION CIRCLE 305279, DENTON, TX
76203-5017 USA
SN 0278-0771
EI 2162-4496
J9 J ETHNOBIOL
JI J. Ethnobiol.
PD MAR
PY 2016
VL 36
IS 1
BP 105
EP 124
PG 20
WC Anthropology; Biology
SC Anthropology; Life Sciences & Biomedicine - Other Topics
GA DO1LP
UT WOS:000377539900007
ER
PT J
AU Shaw, D
Wagelie, J
AF Shaw, Debora
Wagelie, Jennifer
TI Studying artworks and their digital copies: Valuing the artist's aura
SO INTERNATIONAL JOURNAL OF EDUCATION THROUGH ART
LA English
DT Article
DE visual literacy; digital images; original works of art; aura; purpose
AB Digital images extend access to works of art but little is known about of the benefits and limitations of digital copies for instruction. Students in a Museum Studies class viewed either the digital copy or original of two works of art. Regardless of format, the participants formed similar general impressions of the works, although appreciation of the objects' size was difficult with the digital images. Students had difficulty assessing materials and media with both original works and copies. The participants had similar insights and also encountered problems, regardless of whether the work of art was two-or three-dimensional. In describing the advantages of original works, the students also noted the power of the original's aura. Perceived strengths of the digital images included the ability to do research away from the museum (saving travel and time) and to manipulate the images.
C1 [Shaw, Debora] Indiana Univ, Sch Informat & Comp, 1320 E 10th St,LI 011, Bloomington, IN 47405 USA.
[Wagelie, Jennifer] Natl Gallery Art, Washington, DC 20565 USA.
[Wagelie, Jennifer] Indiana Univ Art Museum, Bloomington, IN USA.
[Wagelie, Jennifer] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Wagelie, Jennifer] Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Bloomington, IN USA.
[Wagelie, Jennifer] Sacramento State Univ, Sacramento, CA USA.
[Wagelie, Jennifer] UC Santa Cruz, Santa Cruz, CA USA.
RP Shaw, D (reprint author), Indiana Univ, Sch Informat & Comp, 1320 E 10th St,LI 011, Bloomington, IN 47405 USA.
EM shawd@indiana.edu; jennifer.wagelie@gmail.com
NR 26
TC 1
Z9 1
U1 0
U2 0
PU INTELLECT LTD
PI BRISTOL
PA THE MILL, PARNALL RD, BRISTOL, BS16 3JG, ENGLAND
SN 1743-5234
EI 2040-090X
J9 INT J EDUC ART
JI Int. J. Educ. Art
PD MAR
PY 2016
VL 12
IS 1
BP 57
EP 69
DI 10.1386/eta.12.1.57_1
PG 13
WC Education & Educational Research
SC Education & Educational Research
GA DM7GH
UT WOS:000376525000005
ER
PT J
AU Hintz, ES
AF Hintz, Eric S.
TI A Triumph of Genius: Edwin Land, Polaroid, and the Kodak Patent War.
SO BUSINESS HISTORY REVIEW
LA English
DT Book Review
C1 [Hintz, Eric S.] Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
RP Hintz, ES (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0007-6805
EI 2044-768X
J9 BUS HIST REV
JI Bus. Hist. Rev.
PD SPR
PY 2016
VL 90
IS 1
BP 131
EP 133
DI 10.1017/S000768051600009X
PG 3
WC Business; History Of Social Sciences
SC Business & Economics; Social Sciences - Other Topics
GA DM1GT
UT WOS:000376094100012
ER
PT J
AU Connette, GM
Osbourn, MS
Peterman, WE
AF Connette, Grant M.
Osbourn, Michael S.
Peterman, William E.
TI The Distribution of a Stream-breeding Salamander, Desmognathus ocoee, in
Terrestrial Habitat Suggests the Ecological Importance of Low-order
Streams
SO COPEIA
LA English
DT Article; Proceedings Paper
CT 6th Conference on the Biology of Plethodontid Salamanders
CY MAY 18-20, 2014
CL Univ Tulsa, Tulsa, OK
HO Univ Tulsa
ID SOUTHERN APPALACHIAN SALAMANDERS; HEADWATER STREAMS; RIPARIAN BUFFERS;
LIFE-HISTORY; LARVAL SALAMANDERS; GENUS DESMOGNATHUS; PACIFIC-NORTHWEST;
TIMBER HARVEST; WESTERN OREGON; MANAGEMENT
AB Small headwater streams are a common feature of many forested landscapes, and their integrity is considered critical to the maintenance of water quality and biodiversity within broader drainage networks. Although riparian buffer zones are often established to limit disturbance to stream ecosystems from human land use, various buffer zone management strategies may provide effective protection to certain aquatic or semi-aquatic species while only encompassing a portion of core habitat for other species. Thus, an improved understanding of species distributions within riparian forests can be useful for predicting the overall effectiveness of various forest management practices. In this study, we conducted area-constrained surveys for salamanders at 16 plots within terrestrial habitat. We then employed an information-theoretic (AIC) approach to model selection to quantify the distribution of aquatic-breeding Ocoee Salamanders, Desmognathus ocoee, within terrestrial habitat as a function of stream length, width, and/or proximity within the surrounding landscape. Based on a mechanistic model for salamander counts, we estimated that 95% of Ocoee Salamanders are distributed within 79 m of their stream of origin and that relative abundance should decline exponentially with distance into terrestrial habitat. However, a simple model describing salamander counts as an exponential decay with distance from the nearest stream received the strongest support overall, suggesting that this may represent a good predictive model for the distribution of D. ocoee in terrestrial habitat. Due to the prevalence of headwater streams and seeps which do not appear on topographic maps, protecting 95% of core terrestrial habitat around all stream features would require protecting 59.3% of our study landscape. Models describing the spatial distributions of semi-aquatic organisms within terrestrial habitat can be useful for providing spatially explicit density estimates for species conservation or management efforts.
C1 [Connette, Grant M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Myanmar Program, 1500 Remount Rd, Front Royal, VA 22630 USA.
[Osbourn, Michael S.] Appalachian State Univ, Dept Biol, 171b Rankin Sci West,572 Rivers St, Boone, NC 28608 USA.
[Peterman, William E.] Ohio State Univ, Sch Environm & Nat Resources, 210 Kottman Hall,2021 Coffey Rd, Columbus, OH 43210 USA.
RP Connette, GM (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Myanmar Program, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM grmcco@gmail.com; osbournms@appstate.edu; Peterman.73@osu.edu
RI Peterman, William/H-7809-2013
OI Peterman, William/0000-0001-5229-9268
NR 49
TC 0
Z9 0
U1 5
U2 10
PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS
PI MIAMI
PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200
SW 8TH STREET, MIAMI, FL 33199 USA
SN 0045-8511
EI 1938-5110
J9 COPEIA
JI Copeia
PD MAR
PY 2016
VL 104
IS 1
BP 149
EP 156
DI 10.1643/OT-14-215
PG 8
WC Zoology
SC Zoology
GA DM2OK
UT WOS:000376185900019
ER
PT J
AU Smith, DG
Bowman, IA
AF Smith, David G.
Bowman, Inci A.
TI 50th Anniversary Meeting of ASIH in Vancouver, 1963
SO COPEIA
LA English
DT Editorial Material
C1 [Smith, David G.] Smithsonian Inst, Museum Support Ctr, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA.
[Bowman, Inci A.] Natl Museum Nat Hist, Div Fishes, MRC-159, Washington, DC 20013 USA.
RP Smith, DG (reprint author), Smithsonian Inst, Museum Support Ctr, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA.; Bowman, IA (reprint author), Natl Museum Nat Hist, Div Fishes, MRC-159, Washington, DC 20013 USA.
EM smithd@si.edu; inciabowman@gmail.com
NR 16
TC 1
Z9 1
U1 0
U2 0
PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS
PI MIAMI
PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200
SW 8TH STREET, MIAMI, FL 33199 USA
SN 0045-8511
EI 1938-5110
J9 COPEIA
JI Copeia
PD MAR
PY 2016
VL 104
IS 1
BP 278
EP 285
DI 10.1643/OT-15-388
PG 8
WC Zoology
SC Zoology
GA DM2OK
UT WOS:000376185900033
ER
PT J
AU Jerep, FC
Camelier, P
Malabarba, LR
AF Jerep, Fernando C.
Camelier, Priscila
Malabarba, Luiz R.
TI Serrapinnus zanatae, a new species from the rio Jequitinhonha basin,
Minas Gerais State, Brazil (Teleostei: Characidae: Cheirodontinae)
SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS
LA English
DT Article
ID NORTHEASTERN BRAZIL; GENUS; CHARACIFORMES; MALABARBA
AB Serrapinnus zanatae, new species, is described from the rio Jequitinhonha basin, an eastern Brazilian coastal drainage. It is diagnosed from its congeners by the following combination of characters: presence of premaxillary teeth with 7-9 cusps; 11-13 parallel spatulated ventral procurrent caudal-fin rays; incomplete lateral line; absence of a black blotch on the dorsal fin; absence of a dark longitudinal stripe extending over the pseudotympanum to the caudal peduncle; absence of a black spot on the posteroventral region of the abdomen; caudal-fin spot oval and horizontally elongated not extending to dorsal and ventral margins of the caudal peduncle; sexually dimorphic males without unbranched dorsal-, pelvic-, and anal-fin rays extended as filaments. Serrapinnus zanatae and Aci-nocheirodon melanogramma are the only known cheirodontines to inhabit the rio Jequitinhonha basin.
C1 [Jerep, Fernando C.] Univ Estadual Londrina, Programa Posgrad Ciencias Biol, Dept Biol Anim & Vegetal, Ctr Ciencias Biol, BR-86057970 Londrina, PR, Brazil.
[Jerep, Fernando C.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Camelier, Priscila] Univ Sao Paulo, Museu Zool, Ave Nazare 481,Caixa Postal 42494, BR-04218970 Sao Paulo, SP, Brazil.
[Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, Av Paulo Gama S-N, BR-91501970 Porto Alegre, RS, Brazil.
RP Jerep, FC (reprint author), Univ Estadual Londrina, Programa Posgrad Ciencias Biol, Dept Biol Anim & Vegetal, Ctr Ciencias Biol, BR-86057970 Londrina, PR, Brazil.; Jerep, FC (reprint author), Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM fjerep@gmail.com; pricamelier@gmail.com; malabarb@ufrgs.br
RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016
FU CNPq [453850/2014-6, 300705/2010-7, 477318/2012-6]; FAPESP
[2012/00840-6]
FX We thank A. M. Zanata (UFBA), C. A. Lucena (MCP), C. Pavanelli
(NUPELIA), G. B. Santos, T. C. Pessali (MCNIP), O. Oyakawa (MZUSP), M.
Sabaj Perez (ANSP), M. A. Rogers, K. Swagel (FMNH), R. Vari, J. Clayton
(USNM), D. Catania and J. D. Fong (CAS) for loan of specimens and for
museum and technical support. We are also grateful to A. M. Zanata, B.
Sardeiro, I. S. Penido J. F. Pezzi da Silva, J. O. Birindelli, L. Sousa,
R. Burger, R. E. Reis, R. M. C. Castro, S. L. Jewett, T. A. Barroso, T.
C. Pessali, W. G. Saul, and Departamento de Zoologia (DZ) and MZUSP-USNM
Expeditions for their help during fieldwork and/or to collect the type
material. To J. L. O. Birindelli for photograph of Figure 5a, T. C.
Pessali for Figure 5b, and A. M. Zanata for Figure 7. FCJ research is
supported by CNPq (453850/2014-6) and visit to MCP by CNPq
(504177/2012-5). PC research is supported by FAPESP (2012/00840-6). LRM
research is supported by CNPq (300705/2010-7; 477318/2012-6).
NR 19
TC 0
Z9 0
U1 0
U2 0
PU VERLAG DR FRIEDRICH PFEIL
PI MUNICH
PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY
SN 0936-9902
J9 ICHTHYOL EXPLOR FRES
JI Ichthyol. Explor. Freshw.
PD MAR
PY 2016
VL 26
IS 4
BP 289
EP 298
PG 10
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA DK2CG
UT WOS:000374721600001
ER
PT J
AU Lin, HW
Loeb, A
AF Lin, Henry W.
Loeb, Abraham
TI Scaling relations of halo cores for self-interacting dark matter
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter experiments; dark matter theory; dwarfs galaxies
ID DWARF SPHEROIDAL GALAXIES; MILKY-WAY; DENSITY; EVOLUTION; PROFILES;
COLLAPSE; MODELS
AB Using a simple analytic formalism, we demonstrate that significant dark matter self-interactions produce halo cores that obey scaling relations nearly independent of the underlying particle physics parameters such as the annihilation cross section and the mass of the dark matter particle. For dwarf galaxies, we predict that the core density pc and the core radius r(c) should obey rho(c)r(c) approximate to 41 M(circle dot)pc(-2) with a weak mass dependence similar to M-0.2. Remarkably, such a scaling relation has recently been empirically inferred. Scaling relations involving core mass, core radius, and core velocity dispersion are predicted and agree well with observational data. By calibrating against numerical simulations, we predict the scatter in these relations and find them to be in excellent agreement with existing data. Future observations can test our predictions for different halo masses and redshifts.
C1 [Lin, Henry W.; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
RP Lin, HW; Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
EM henrylin@college.harvard.edu; aloeb@cfa.harvard.edu
OI Lin, Henry/0000-0003-2767-6142
FU NSF [AST-1312034]
FX This work was supported in part by NSF grant AST-1312034.
NR 31
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD MAR
PY 2016
IS 3
AR 009
DI 10.1088/1475-7516/2016/03/009
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DL4LO
UT WOS:000375608200011
ER
PT J
AU Kimura, T
Kraft, RP
Elsner, RF
Branduardi-Raymont, G
Gladstone, GR
Tao, C
Yoshioka, K
Murakami, G
Yamazaki, A
Tsuchiya, F
Vogt, MF
Masters, A
Hasegawa, H
Badman, SV
Roediger, E
Ezoe, Y
Dunn, WR
Yoshikawa, I
Fujimoto, M
Murray, SS
AF Kimura, T.
Kraft, R. P.
Elsner, R. F.
Branduardi-Raymont, G.
Gladstone, G. R.
Tao, C.
Yoshioka, K.
Murakami, G.
Yamazaki, A.
Tsuchiya, F.
Vogt, M. F.
Masters, A.
Hasegawa, H.
Badman, S. V.
Roediger, E.
Ezoe, Y.
Dunn, W. R.
Yoshikawa, I.
Fujimoto, M.
Murray, S. S.
TI Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and
Hisaki satellite
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Jupiter; X-ray; magnetosphere
ID KELVIN-HELMHOLTZ VORTICES; PHOTON IMAGING CAMERA; SOLAR-WIND;
RELATIVISTIC ELECTRONS; SATURNS MAGNETOPAUSE; EMISSION-SPECTRA;
MAGNETIC-FIELD; ULYSSES RADIO; MAGNETOSPHERE; BURSTS
AB Jupiter's X-ray auroral emission in the polar cap region results from particles which have undergone strong field-aligned acceleration into the ionosphere. The origin of precipitating ions and electrons and the time variability in the X-ray emission are essential to uncover the driving mechanism for the high-energy acceleration. The magnetospheric location of the source field line where the X-ray is generated is likely affected by the solar wind variability. However, these essential characteristics are still unknown because the long-term monitoring of the X-rays and contemporaneous solar wind variability has not been carried out. In April 2014, the first long-term multiwavelength monitoring of Jupiter's X-ray and EUV auroral emissions was made by the Chandra X-ray Observatory, XMM-Newton, and Hisaki satellite. We find that the X-ray count rates are positively correlated with the solar wind velocity and insignificantly with the dynamic pressure. Based on the magnetic field mapping model, a half of the X-ray auroral region was found to be open to the interplanetary space. The other half of the X-ray auroral source region is magnetically connected with the prenoon to postdusk sector in the outermost region of the magnetosphere, where the Kelvin-Helmholtz (KH) instability, magnetopause reconnection, and quasiperiodic particle injection potentially take place. We speculate that the high-energy auroral acceleration is associated with the KH instability and/or magnetopause reconnection. This association is expected to also occur in many other space plasma environments such as Saturn and other magnetized rotators.
C1 [Kimura, T.; Yoshioka, K.; Murakami, G.; Yamazaki, A.; Hasegawa, H.; Fujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
[Kimura, T.] RIKEN, Nishina Ctr Accelerator Based Sci, Saitama, Japan.
[Kimura, T.; Kraft, R. P.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Elsner, R. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Branduardi-Raymont, G.; Dunn, W. R.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Gladstone, G. R.] SW Res Inst, Dept Space Studies, Boulder, CO USA.
[Tao, C.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Tsuchiya, F.] Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Sendai, Miyagi 980, Japan.
[Vogt, M. F.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Masters, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Fac Nat Sci, London, England.
[Badman, S. V.] Univ Lancaster, Dept Phys, Lancaster, England.
[Roediger, E.] Univ Hamburg, Hamburger Sternwarte, Hamburg, Germany.
[Ezoe, Y.] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Yoshikawa, I.] Univ Tokyo, Dept Complex Sci & Engn, Chiba, Japan.
[Fujimoto, M.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 152, Japan.
RP Kimura, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.; Kimura, T (reprint author), RIKEN, Nishina Ctr Accelerator Based Sci, Saitama, Japan.; Kimura, T (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM tomoki.kimura@riken.jp
RI Hasegawa, Hiroshi/A-1192-2007; Vogt, Marissa/C-6237-2014
OI Hasegawa, Hiroshi/0000-0002-1172-021X; Vogt, Marissa/0000-0003-4885-8615
FU Japan Society for the Promotion of Science (JSPS)
FX T.K. was supported by a grant-in-aid for Scientific Research from the
Japan Society for the Promotion of Science (JSPS). The data of Hisaki
satellite are archived in the Data Archives and Transmission System
(DARTS) JAXA. Individuals may request the data by writing to Timoki
Kimura (tomoki.kimura@riken.jp).
NR 65
TC 2
Z9 2
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2308
EP 2320
DI 10.1002/2015JA021893
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900031
ER
PT J
AU Halfwerk, W
Lea, AM
Guerra, MA
Page, RA
Ryan, MJ
AF Halfwerk, W.
Lea, A. M.
Guerra, M. A.
Page, R. A.
Ryan, M. J.
TI Vocal responses to noise reveal the presence of the Lombard effect in a
frog
SO BEHAVIORAL ECOLOGY
LA English
DT Article
DE ambient noise; eavesdropping; Lombard effect; sexual selection; signal
plasticity
ID FEMALE TUNGARA FROGS; ACOUSTIC COMMUNICATION; ADVERTISEMENT CALLS;
ANTHROPOGENIC NOISE; TRAFFIC NOISE; PHYSALAEMUS-PUSTULOSUS;
HYPEROLIUS-MARMORATUS; ENVIRONMENTAL NOISE; MATING SIGNALS; MATE CHOICE
AB Many animal communication systems have evolved signal flexibility depending on environmental conditions. A common strategy of vocal communication is to increase amplitude in response to increasing noise levels. This phenomenon, known as the Lombard effect, is a widespread trait among mammals and birds. Anurans are a major group with many species that rely heavily on acoustic signals for sexual communication. Although these species often communicate in noisy environments, the presence of the Lombard effect in frogs remains unclear. We exposed male tungara frogs (Physalaemus pustulosus) to different noises with and without playback of conspecific calls. Males increased call amplitude, call rate, and call complexity in response to low-frequency noise (overlapping the species' call range) but not to high-frequency (nonoverlapping) noise. Vocal amplitude increased linearly with noise level demonstrating that tungara frogs exhibit the Lombard effect, and we discuss why different frog species may differ in their control over vocal amplitudes. Furthermore, we found the overall effect of noise to be similar to the effect of conspecific call playback. We speculate that vocal amplitude control may have evolved primarily as a response to increased competition at the cocktail party, similar to the way humans raise their voice when in a heated debate, and subsequently as a strategy to deal with background noise more generally.
C1 [Halfwerk, W.; Page, R. A.; Ryan, M. J.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Halfwerk, W.; Lea, A. M.; Guerra, M. A.; Ryan, M. J.] Univ Texas Austin, Dept Integrat Biol, 1 Univ Stn, Austin, TX 78712 USA.
[Halfwerk, W.] Vrije Univ Amsterdam, Dept Ecol Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands.
RP Halfwerk, W (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.; Halfwerk, W (reprint author), Univ Texas Austin, Dept Integrat Biol, 1 Univ Stn, Austin, TX 78712 USA.; Halfwerk, W (reprint author), Vrije Univ Amsterdam, Dept Ecol Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands.
EM w.h.halfwerk@vu.nl
FU Smithsonian Institute fellowship; National Science Foundation [IBN
0517328]
FX This work was supported by a Smithsonian Institute fellowship to W.H., a
graduate research fellowship of the National Science Foundation to
A.M.L., and an National Science Foundation grant (grant number: IBN
0517328) to M.J.R. and R.A.P.
NR 68
TC 7
Z9 7
U1 12
U2 26
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
EI 1465-7279
J9 BEHAV ECOL
JI Behav. Ecol.
PD MAR-APR
PY 2016
VL 27
IS 2
BP 669
EP 676
DI 10.1093/beheco/arv204
PG 8
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA DL1NL
UT WOS:000375398800042
ER
PT J
AU Aona, LYS
Faden, RB
Bittrich, V
Amaral, MDE
AF Aona, Lidyanne Y. S.
Faden, Robert B.
Bittrich, Volker
Amaral, Maria do Carmo E.
TI Four new species of Dichorisandra (Commelinaceae) endemic from Bahia
State, Brazil
SO BRITTONIA
LA English
DT Article
DE Atlantic Forest; conservation; Dichorisandrinae; southern Bahia
ID FORESTS
AB The four new species described here occur in the Brazilian state of Bahia. Dichorisandra marantoides can be distinguished from other species of the genus by its chartaceous longitudinally ribbed leaves, flowers with five stamens and anthers opening introrsely by slits (being functionally poricidal). Dichorisandra bahiensis is similar to D. tejucensis due to the habit and leaf and flower morphology. However, the two species can be distinguished by the inflorescence, which in D. bahiensis is always positioned at the apex of the stems, perforating the sheath of the lowermost leaf of the lateral branch. Dichorisandra saxatilis resembles D. glaziovii by the morphology and color of anthers, but differs by presence of six stamens, the leaves regularly dispersed along the stem, their laminas glabrous on both sides, with the adaxial surface always green, never with white stripes. Dichorisandra leucosepala also can be distinguished from other species of the genus by white (rarely purplish at the apex), carnose sepals, six stamens with anthers opening by a single pore with purplish pollen sacs. Illustrations of the species, comparisons with similar species, discussions of diagnostic characters and conservation status of the new species are presented.
C1 [Aona, Lidyanne Y. S.] Univ Fed Reconcavo Bahia, Ctr Ciencias Agr Ambientais & Biol, Campus Univ,Rua Rui Barbosa 710, BR-44380000 Cruz das Almas, BA, Brazil.
[Faden, Robert B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA.
[Bittrich, Volker] Rua Dr Mario de Nucci 500, BR-13083290 Campinas, SP, Brazil.
[Amaral, Maria do Carmo E.] Univ Estadual Campinas UNICAMP, Dept Biol Vegetal, Inst Biol, Caixa Postal 6109, BR-13083970 Campinas, SP, Brazil.
RP Aona, LYS (reprint author), Univ Fed Reconcavo Bahia, Ctr Ciencias Agr Ambientais & Biol, Campus Univ,Rua Rui Barbosa 710, BR-44380000 Cruz das Almas, BA, Brazil.
EM lidyanne.aona@gmail.com
OI Aona, Lidyanne/0000-0001-8477-5791
FU Research Support Foundation of Sao Paulo State-FAPESP [03/06634-0];
Fundacao Botanica Margaret Mee; CNPq; Smithsonian Institution,
Washington
FX This study is part of a Ph.D. thesis by the first author for the
graduate course in Plant Biology at the Universidade Estadual de
Campinas (Sao Paulo, Brazil). This work was supported by the Research
Support Foundation of Sao Paulo State-FAPESP (process no 03/06634-0) and
the Fundacao Botanica Margaret Mee for a fellowship to study at the
Royal Botanic Gardens, Kew. MCEA thanks CNPq for a research grant, and
the Smithsonian Institution, Washington, for a grant from the Short Term
Visitor Program. We are grateful the curators and staff at ALCB, CEPEC,
FURB, G, HUEFS, HURB, NY, K, RB, SPF, SP, US and UEC for providing
access to their collections; Carla Lima for the line drawings, L. C.
Marinho for the graphical support, A. M. Amorim for the photo of
Dichorisandra leucosepala and Lea M. E. Amaral for her careful help in
cultivating the plants used in this research.
NR 16
TC 1
Z9 2
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0007-196X
EI 1938-436X
J9 BRITTONIA
JI Brittonia
PD MAR
PY 2016
VL 68
IS 1
BP 61
EP 73
DI 10.1007/s12228-015-9397-x
PG 13
WC Plant Sciences
SC Plant Sciences
GA DL1UH
UT WOS:000375417600007
ER
PT J
AU Williams, M
Zalasiewicz, J
Waters, CN
Edgeworth, M
Bennett, C
Barnosky, AD
Ellis, EC
Ellis, MA
Cearreta, A
Haff, PK
do Sul, JAI
Leinfelder, R
McNeill, JR
Odada, E
Oreskes, N
Revkin, A
Richter, DD
Steffen, W
Summerhayes, C
Syvitski, JP
Vidas, D
Wagreich, M
Wing, SL
Wolfe, AP
An, ZS
AF Williams, Mark
Zalasiewicz, Jan
Waters, Colin N.
Edgeworth, Matt
Bennett, Carys
Barnosky, Anthony D.
Ellis, Erle C.
Ellis, Michael A.
Cearreta, Alejandro
Haff, Peter K.
Ivar do Sul, Juliana A.
Leinfelder, Reinhold
McNeill, John R.
Odada, Eric
Oreskes, Naomi
Revkin, Andrew
Richter, Daniel deB
Steffen, Will
Summerhayes, Colin
Syvitski, James P.
Vidas, Davor
Wagreich, Michael
Wing, Scott L.
Wolfe, Alexander P.
An Zhisheng
TI The Anthropocene: a conspicuous stratigraphical signal of anthropogenic
changes in production and consumption across the biosphere
SO EARTHS FUTURE
LA English
DT Review
ID NET PRIMARY PRODUCTION; HUMAN APPROPRIATION; MASS EXTINCTION; FOSSIL
RECORD; CARBON-CYCLE; NITROGEN-CYCLE; FIRE REGIMES; LAND PLANTS;
EVOLUTION; RADIATION
AB Biospheric relationships between production and consumption of biomass have been resilient to changes in the Earth system over billions of years. This relationship has increased in its complexity, from localized ecosystems predicated on anaerobic microbial production and consumption to a global biosphere founded on primary production from oxygenic photoautotrophs, through the evolution of Eukarya, metazoans, and the complexly networked ecosystems of microbes, animals, fungi, and plants that characterize the Phanerozoic Eon (the last similar to 541 million years of Earth history). At present, one species, Homo sapiens, is refashioning this relationship between consumption and production in the biosphere with unknown consequences. This has left a distinctive stratigraphy of the production and consumption of biomass, of natural resources, and of produced goods. This can be traced through stone tool technologies and geochemical signals, later unfolding into a diachronous signal of technofossils and human bioturbation across the planet, leading to stratigraphically almost isochronous signals developing by the mid-20th century. These latter signals may provide an invaluable resource for informing and constraining a formal Anthropocene chronostratigraphy, but are perhaps yet more important as tracers of a biosphere state that is characterized by a geologically unprecedented pattern of global energy flow that is now pervasively influenced and mediated by humans, and which is necessary for maintaining the complexity of modern human societies.
C1 [Williams, Mark; Zalasiewicz, Jan; Bennett, Carys] Univ Leicester, Dept Geol, Leicester LE1 7RH, Leics, England.
[Waters, Colin N.; Ellis, Michael A.] British Geol Survey, Ctr Environm Sci, Nottingham NG12 5GG, England.
[Edgeworth, Matt] Univ Leicester, Sch Archaeol & Ancient Hist, Leicester, Leics, England.
[Barnosky, Anthony D.] Univ Calif Berkeley, Museum Vertebrate Zool, Museum Paleontol, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Ellis, Erle C.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21228 USA.
[Cearreta, Alejandro] Univ Pais Vasco UPV EHU, Fac Ciencia & Tecnol, Dept Estratig & Paleontol, Bilbao, Spain.
[Haff, Peter K.; Richter, Daniel deB] Duke Univ, Nicholas Sch Environm, Div Earth & Ocean Sci, Durham, NC 27708 USA.
[Leinfelder, Reinhold] Free Univ Berlin, Dept Geol Sci, Berlin, Germany.
[McNeill, John R.] Georgetown Univ, Washington, DC USA.
[Odada, Eric] Univ Nairobi, Dept Geol, Nairobi, Kenya.
[Oreskes, Naomi] Harvard Univ, Dept Hist Sci, Cambridge, MA 02138 USA.
[Revkin, Andrew] Pace Univ, Dyson Coll Inst Sustainabil & Environm, Pleasantville, NY USA.
[Steffen, Will] Australian Natl Univ, Canberra, ACT, Australia.
[Summerhayes, Colin] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England.
[Syvitski, James P.] Univ Colorado, Boulder Campus, Boulder, CO 80309 USA.
[Vidas, Davor] Fridtjof Nansen Inst Polhogda, Marine Affairs & Law Sea Programme, Lysaker, Norway.
[Wagreich, Michael] Univ Vienna, Dept Geodynam & Sedimentol, Vienna, Austria.
[Wing, Scott L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Wolfe, Alexander P.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2M7, Canada.
[An Zhisheng] Chinese Acad Sci, Inst Earth Environm, State Key Lab Loess & Quaternary Geol, Xian, Peoples R China.
RP Williams, M (reprint author), Univ Leicester, Dept Geol, Leicester LE1 7RH, Leics, England.
EM mri@le.ac.uk
RI AN, Zhisheng/F-8834-2012;
OI Leinfelder, Reinhold/0000-0002-4107-2161; Cearreta,
Alejandro/0000-0003-0100-1454
NR 148
TC 1
Z9 1
U1 20
U2 39
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD MAR
PY 2016
VL 4
IS 3
BP 34
EP 53
DI 10.1002/2015EF000339
PG 20
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA DK3YP
UT WOS:000374853600001
ER
PT J
AU Lacher, I
Schwartz, MW
AF Lacher, Iara
Schwartz, Mark W.
TI Empirical test on the relative climatic sensitivity between individuals
of narrowly and broadly distributed species
SO ECOSPHERE
LA English
DT Article
DE Clarkia gracilis ssp tracyi; Clarkia purpurea; climate change; Mimulus
guttatus; Mimulus nudatus; range size; sensitivity; species distribution
models; vulnerability
ID MIMULUS-GUTTATUS; RANGE-SIZE; DISTRIBUTION MODELS; EXTINCTION RISK;
BIODIVERSITY CONSERVATION; VEGETATION DISTRIBUTION; PHENOTYPIC
PLASTICITY; TEMPORAL VARIABILITY; SERPENTINE TOLERANCE; CHANGE
ADAPTATION
AB Climate change is already influencing global ecology, exacerbating human-induced biodiversity loss with potentially devastating results. A first step to addressing climate change impacts on conservation is to better understand how and to what extent species will be affected. Species with smaller geographic distributions are commonly perceived to be at highest risk of extinction. However, estimates of species vulnerability are frequently based on simplifying assumptions regarding climatic tolerance, usually arrived at through the use of models that associate mean spatial or temporal climate values with species distributions. Model estimated climatic tolerances may be improved by incorporating either finer spatial or temporal resolutions and/or additional distribution-limiting factors like dispersal, habitat connectivity, and species interactions. However, the underlying assumption that species-level climatic reflect individual tolerances can skew vulnerability estimates toward over-or underestimation. We use empirically derived fitness reaction norms of biomass and seed pod count to estimate the relative sensitivity of individuals of broadly distributed (BD) and narrowly distributed (ND) species across temperature and water gradients. Temperature and water treatments were based on local climate station data and IPCC projections of climatic change. On the basis of fitness reaction norms, we infer relative vulnerability to examine the assumption that ND species are relatively more vulnerable to climatic change than BD species. Study species included the BD Mimulus guttatus and Clarkia purpurea and the ND Mimulus nudatus and Clarkia gracilis ssp. tracyi. Compared to M.nudatus (ND), individuals of M.guttatus (BD) exhibited biomass responses that were significantly more sensitive to temperature and seed pod count responses that were significantly more sensitive to water and temperature. Conversely, compared to C.purpurea (BD), C.gracilis ssp. tracyi (ND) individuals exhibited biomass and seed pod count responses that were significantly more sensitive to temperature. In addition, we measured unexpected positive responses from both Clarkia species to increases in temperature. Our results support the idea that, when examined at a local scale, the size of a species' geographic distribution does not necessarily correlate to climate change vulnerability.
C1 [Lacher, Iara; Schwartz, Mark W.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA.
[Schwartz, Mark W.] Univ Calif Davis, John Muir Inst Environm, Davis, CA 95616 USA.
[Lacher, Iara] Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
RP Lacher, I (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM LacherI@si.edu
RI Schwartz, Mark/G-1066-2011
OI Schwartz, Mark/0000-0002-3739-6542
FU California Native Plant Society; UC Davis; John Muir Institute of the
Environment
FX We thank R. Hijmans, K. Rice, T. Lacher, C. Peters, and C. Dolanc for
helpful comments on this manuscript; all the UC Davis undergraduates who
painstakingly monitored our experiments; and Paul Aigner and Cathy
Koehler for field support. Funding was provided by the California Native
Plant Society, two Jastro Shields Research Awards from UC Davis, and the
John Muir Institute of the Environment.
NR 62
TC 0
Z9 0
U1 0
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2150-8925
J9 ECOSPHERE
JI Ecosphere
PD MAR
PY 2016
VL 7
IS 3
AR e01227
DI 10.1002/ecs2.1227
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA DK4OB
UT WOS:000374896800006
ER
PT J
AU O'Bryan, CJ
Homyack, JA
Baldwin, RF
Kanno, Y
Harrison, AL
AF O'Bryan, C. J.
Homyack, J. A.
Baldwin, R. F.
Kanno, Y.
Harrison, A. -L.
TI Novel habitat use supports population maintenance in a reconfigured
landscape
SO ECOSPHERE
LA English
DT Article
DE behavioral plasticity; Clemmys guttata; ditch; habitat selection;
intensive forestry; plantation; reconfigured landscape; spatial ecology;
spotted turtle
ID TURTLES CLEMMYS-GUTTATA; SOUTHERN UNITED-STATES; SPOTTED TURTLES;
LOGISTIC-REGRESSION; ROAD MORTALITY; UTILIZATION DISTRIBUTIONS; SMALL
WETLANDS; COASTAL-PLAIN; HOME RANGES; SELECTION
AB Given the limited scope of unaltered, protected areas in most regions, understanding the contributions to imperiled species conservation by landscapes in which habitat elements have been reconfigured is critical. Commercial forestry has been a driver of altered structure and composition of forests and of distribution and character of aquatic systems. In eastern North America, extensive historical wetland drainage reconfigured hydrologic environments from low-gradient wet flats and isolated wetlands to connected networks of linear ditches. Landscapes where both uplands and aquatic environments differ from historic conditions may affect most ecological aspects of semi-aquatic species, including reptiles. Our objective was to determine if habitat selection and use decisions by spotted turtles (Clemmys guttata), a rare semi-aquatic species, supported population maintenance in a reconfigured forest landscape in eastern North Carolina, USA. We captured 280 individuals and radiomarked 31 adults to examine habitat selection at multiple spatial scales with paired logistic regression, movements and home ranges with location data and utilization distributions (UDs), survival with a known-fate model, and abundance with N-mixture modeling. Across local and landscape scales, turtles selected features associated with ditches despite abundant, more natural aquatic depressions across the study area. Habitat metrics describing understory closure and substrate characteristics were important at local scales, and closed canopy forest and habitat heterogeneity was positively associated with activity areas at landscape-scale spatial grains. Both movements and home ranges were centered on ditches, and turtles exploited ditches to access mates, nest sites, or uplands for estivation. In this highly reconfigured landscape, this species appeared to have sufficient behavioral plasticity to acquire key resources contributing to high survival and an abundant population. Isolation from road traffic and collection, both which negatively affect turtles elsewhere, was facilitated by limited public access. Our results suggest that conservation and management of rare species should not rely solely on habitat information gained from studies in more pristine areas because such results may not demonstrate the range in variation in behavior that might allow persistence in novel environments, absent key threats.
C1 [O'Bryan, C. J.; Baldwin, R. F.; Kanno, Y.] Clemson Univ, Dept Forestry & Environm Conservat, 132 Lehotsky Hall, Clemson, SC 29634 USA.
[Homyack, J. A.] Weyerhaeuser Co, 1785 Weyerhaeuser Rd, Vanceboro, NC 28586 USA.
[Harrison, A. -L.] Clemson Univ, Inst Parks, 263 Lehotsky Hall, Clemson, SC 29634 USA.
RP O'Bryan, CJ (reprint author), Clemson Univ, Dept Forestry & Environm Conservat, 132 Lehotsky Hall, Clemson, SC 29634 USA.; O'Bryan, CJ (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,MRC 5503, Washington, DC 20013 USA.
EM obryancj@gmail.com
OI O'Bryan, Christopher/0000-0002-6472-6957
FU Weyerhaeuser Company; North Carolina Wildlife Resources Commission;
National Council for Air and Stream Improvement; Clemson University
Department of Forestry and Environmental Conservation
FX We thank E. Abernethy and L. Paden for field assistance. J. W. Coffey,
J. Hall, T. B. Wigley, and T. Gorman contributed to study design and
analyses and J. Grant, A. J. Kroll, and J. Litzgus improved earlier
drafts. Funding was provided by Weyerhaeuser Company, North Carolina
Wildlife Resources Commission, National Council for Air and Stream
Improvement, and Clemson University Department of Forestry and
Environmental Conservation.
NR 73
TC 2
Z9 2
U1 11
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2150-8925
J9 ECOSPHERE
JI Ecosphere
PD MAR
PY 2016
VL 7
IS 3
AR e01228
DI 10.1002/ecs2.1228
PG 15
WC Ecology
SC Environmental Sciences & Ecology
GA DK4OB
UT WOS:000374896800007
ER
PT J
AU Olson, SL
Wiley, JW
AF Olson, Storrs L.
Wiley, James W.
TI THE BLUE -HEADED QUAIL-DOVE (STARNOENAS CYANOCEPHALA): AN AUSTRALASIAN
DOVE MAROONED IN CUBA
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
DE anatomy; behavior; Columbidae; Geophaps; Geotrygon; paleontology;
Starnoenadinae; zoogeography
ID EARLY OLIGOCENE; EARLY MIOCENE; COLUMBIDAE; TODIDAE; DISPLAY; PIGEON;
AVES; GERMANY
AB We review the taxonomic history, external Morphology, anatomy, behavior, distribution, and zoogeography of the Blue-headed Quail-Dove (Starnoenas cyanocephala), which is endemic to Cuba, and conclude that it is completely unlike any other New World member of the Columbidae. It presents a mosaic of characters shared with various genera in Australasia but is perhaps most similar to the Australian genus Geophaps and related terrestrial pigeons. The Blue headed Quail-Dove should be placed in its own subfamily, Starnoenadinae, until its relationships with Australasian genera can be refined by additional data including molecular. We recommend that the English name be changed to Blue-headed Partridge-Dove.
C1 [Olson, Storrs L.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
[Wiley, James W.] POB 64, Marion Stn, MD 21838 USA.
RP Olson, SL (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.; Wiley, JW (reprint author), POB 64, Marion Stn, MD 21838 USA.
EM olsons@si.edu; jwwiley@mail.umes.edu
NR 81
TC 0
Z9 0
U1 0
U2 0
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
EI 1938-5447
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD MAR
PY 2016
VL 128
IS 1
BP 1
EP 21
PG 21
WC Ornithology
SC Zoology
GA DK9HR
UT WOS:000375242000001
ER
PT J
AU Anderson, FE
Bergamaschi, B
Sturtevant, C
Knox, S
Hastings, L
Windham-Myers, L
Detto, M
Hestir, EL
Drexler, J
Miller, RL
Matthes, JH
Verfaillie, J
Baldocchi, D
Snyder, RL
Fujii, R
AF Anderson, Frank E.
Bergamaschi, Brian
Sturtevant, Cove
Knox, Sara
Hastings, Lauren
Windham-Myers, Lisamarie
Detto, Matteo
Hestir, Erin L.
Drexler, Judith
Miller, Robin L.
Matthes, Jaclyn Hatala
Verfaillie, Joseph
Baldocchi, Dennis
Snyder, Richard L.
Fujii, Roger
TI Variation of energy and carbon fluxes from a restored temperate
freshwater wetland and implications for carbon market verification
protocols
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE wetlands; eddy covariance; carbon dioxide; methane; carbon market;
global warming potential
ID SAN-JOAQUIN DELTA; DISSOLVED ORGANIC-CARBON; PATH GAS ANALYZERS; METHANE
EMISSION; EDDY COVARIANCE; DIOXIDE EXCHANGE; CO2 FLUX; ECOSYSTEM
RESPIRATION; PEATLAND RESTORATION; PRIMARY PRODUCTIVITY
AB Temperate freshwater wetlands are among the most productive terrestrial ecosystems, stimulating interest in using restored wetlands as biological carbon sequestration projects for greenhouse gas reduction programs. In this study, we used the eddy covariance technique to measure surface energy carbon fluxes from a constructed, impounded freshwater wetland during two annual periods that were 8years apart: 2002-2003 and 2010-2011. During 2010-2011, we measured methane (CH4) fluxes to quantify the annual atmospheric carbon mass balance and its concomitant influence on global warming potential (GWP). Peak growing season fluxes of latent heat and carbon dioxide (CO2) were greater in 2002-2003 compared to 2010-2011. In 2002, the daily net ecosystem exchange reached as low as -10.6gCm(-2)d(-1), which was greater than 3 times the magnitude observed in 2010 (-2.9gCm(-2)d(-1)). CH4 fluxes during 2010-2011 were positive throughout the year and followed a strong seasonal pattern, ranging from 38.1mgCm(-2)d(-1) in the winter to 375.9mgCm(-2)d(-1) during the summer. The results of this study suggest that the wetland had reduced gross ecosystem productivity in 2010-2011, likely due to the increase in dead plant biomass (standing litter) that inhibited the generation of new vegetation growth. In 2010-2011, there was a net positive GWP (675.3gCm(-2)yr(-1)), and when these values are evaluated as a sustained flux, the wetland will not reach radiative balance even after 500years.
C1 [Anderson, Frank E.; Bergamaschi, Brian; Drexler, Judith; Miller, Robin L.; Fujii, Roger] US Geol Survey, Sacramento, CA USA.
[Sturtevant, Cove; Knox, Sara; Matthes, Jaclyn Hatala; Verfaillie, Joseph; Baldocchi, Dennis] Univ Calif Berkeley, Ecosyst Sci Div, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Hastings, Lauren] Delta Stewardship Council, Sacramento, CA USA.
[Windham-Myers, Lisamarie] US Geol Survey, 345 Middlefield Rd, Menlo Pk, CA 94025 USA.
[Detto, Matteo] Smithsonian Trop Res Inst, Panama City, Panama.
[Hestir, Erin L.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
[Snyder, Richard L.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
RP Anderson, FE (reprint author), US Geol Survey, Sacramento, CA USA.
EM fanders@usgs.gov
RI Baldocchi, Dennis/A-1625-2009;
OI Baldocchi, Dennis/0000-0003-3496-4919; Matthes,
Jaclyn/0000-0001-8999-8062; Bergamaschi, Brian/0000-0002-9610-5581;
Sturtevant, Cove/0000-0002-0341-3228
FU United States Geological Survey (USGS) Land Carbon Program; California's
Department of Water Resources (DWR) Levee Program; USGS Cooperative
Water Program
FX Flux data from the restored wetland on Twitchell Island can be made
available upon request. In the near future, we plan to make the data
accessible through Ameriflux program (http://ameriflux.ornl.gov). This
research was supported by the United States Geological Survey (USGS)
Land Carbon Program, California's Department of Water Resources (DWR)
Levee Program, and the USGS Cooperative Water Program. We specifically
thank Curt Schmutte who helped conceive this wetland experiment. We are
grateful for the independent USGS peer reviewers (Barclay Shoemaker) and
anonymous journal reviewers for their valuable comments and edits. We
would also like to recognize and thank John Franco Saraceno for his
insightful discussions about uncertainty analysis and Matlab programing,
as well as the many other scientists who have supported and advanced the
science of this restored freshwater wetland over the past two decades.
Any use of trade, firm, or product names is for descriptive purposes
only and does not imply endorsement by the U.S. Government.
NR 76
TC 1
Z9 1
U1 18
U2 43
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR
PY 2016
VL 121
IS 3
BP 777
EP 795
DI 10.1002/2015JG003083
PG 19
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DJ6TD
UT WOS:000374345000011
ER
PT J
AU Zeitlin, C
Case, AW
Schwadron, NA
Spence, HE
Mazur, JE
Joyce, CJ
Looper, MD
Jordan, A
Rios, RR
Townsend, LW
Kasper, JC
Blake, JB
Smith, S
Wilson, J
Iwata, Y
AF Zeitlin, C.
Case, A. W.
Schwadron, N. A.
Spence, H. E.
Mazur, J. E.
Joyce, C. J.
Looper, M. D.
Jordan, A.
Rios, R. R.
Townsend, L. W.
Kasper, J. C.
Blake, J. B.
Smith, S.
Wilson, J.
Iwata, Y.
TI Solar modulation of the deep space galactic cosmic ray lineal energy
spectrum measured by CRaTER, 2009-2014
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE solar modulation; CRaTER; galactic cosmic rays
ID RADIATION ENVIRONMENT; MICROELECTRONICS CODE; INSTRUMENT; PARTICLES;
REVISION
AB The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) is an energetic particle detector flying aboard the Lunar Reconnaissance Orbiter. Since arriving at the Moon in 2009, CRaTER has observed the deep solar minimum of solar cycle 23, the ascending phase of cycle 24, the very weak maximum of cycle 24, and in recent months, what appears to be the start of the descending phase of cycle 24. In earlier work, we presented lineal energy spectra of galactic cosmic rays (GCRs) at solar minimum for different shielding depths. The long period of CRaTER observations allows us to study the evolution of these spectra as a function of solar modulation. As solar modulation increases, the total flux of GCRs decreases, and lower-energy ions are preferentially removed from the spectrum of ions that arrive in the inner heliosphere. These effects lead to modest variations in the lineal energy spectrum as a function of time. GCR fluxes at the 2009/2010 solar minimum were high by historical standards and at solar maximum remained high compared to earlier maxima.
C1 [Zeitlin, C.] SW Res Inst, Dept Earth Oceans & Space, Durham, NH USA.
[Zeitlin, C.; Rios, R. R.] Lockheed Martin Informat Syst & Global Solut, Houston, TX USA.
[Case, A. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Schwadron, N. A.; Spence, H. E.; Joyce, C. J.; Jordan, A.; Smith, S.; Wilson, J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Mazur, J. E.; Looper, M. D.; Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA.
[Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Iwata, Y.] Natl Inst Radiol Sci, Chiba 260, Japan.
RP Zeitlin, C (reprint author), SW Res Inst, Dept Earth Oceans & Space, Durham, NH USA.; Zeitlin, C (reprint author), Lockheed Martin Informat Syst & Global Solut, Houston, TX USA.
EM cary.j.zeitlin@nasa.gov
FU Southwest Research Institute [12-053]; University of New Hampshire;
University of New Hampshire under NASA CRaTER [NNG11PA03C]
FX This work was supported by Southwest Research Institute under agreement
12-053 with the University of New Hampshire and by the University of New
Hampshire under the NASA CRaTER contract NNG11PA03C. We thank Daniel
Matthia of the German Aerospace Agency (DLR) and Serkan Golge of the
NASA-JSC Space Radiation Analysis Group for helpful discussions and for
providing the GCR flux calculations in Table 1. Full CRaTER data sets,
both raw and calibrated, are publicly available for download via the
NASA Planetary Data System (PDS). The data are hosted at the Plasma
Planetary Interactions Node, http://ppi.pds.nasa.gov/index.jsp.
NR 30
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAR
PY 2016
VL 14
IS 3
BP 247
EP 258
DI 10.1002/2015SW001314
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DK1UB
UT WOS:000374698800006
ER
PT J
AU Williamson, CE
Overholt, EP
Brentrup, JA
Pilla, RM
Leach, TH
Schladow, SG
Warren, JD
Urmy, SS
Sadro, S
Chandra, S
Neale, PJ
AF Williamson, Craig E.
Overholt, Erin P.
Brentrup, Jennifer A.
Pilla, Rachel M.
Leach, Taylor H.
Schladow, S. Geoffrey
Warren, Joseph D.
Urmy, Samuel S.
Sadro, Steven
Chandra, Sudeep
Neale, Patrick J.
TI Sentinel responses to droughts, wildfires, and floods: effects of UV
radiation on lakes and their ecosystem services
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Article
ID ULTRAVIOLET-RADIATION; UNITED-STATES; EXTREME; DAPHNIA; CLIMATE; CARBON;
FISH; MATTER; WATERS; TAHOE
AB Environmental drivers such as climate change are responsible for extreme events that are critically altering freshwater resources across the planet. In the continental US, these events range from increases in the frequency and duration of droughts and wildfires in the West, to increasing precipitation and floods that are turning lakes and reservoirs brown in the East. Such events transform and transport organic carbon in ways that affect the exposure of ecosystems to ultraviolet (UV) radiation and visible light, with important implications for ecosystem services. Organic matter dissolved in storm runoff or released as black carbon in smoke selectively reduces UV radiation exposure. In contrast, droughts generally increase water transparency, so that UV radiation and visible light penetrate to greater depths. These shifts in water transparency alter the potential for solar disinfection of waterborne parasites, the production of carcinogenic disinfection byproducts in drinking water, and the vertical distribution of zooplankton that are a critical link in aquatic food webs.
C1 [Williamson, Craig E.; Overholt, Erin P.; Brentrup, Jennifer A.; Pilla, Rachel M.; Leach, Taylor H.] Miami Univ, Dept Biol, Oxford, OH 45056 USA.
[Schladow, S. Geoffrey] Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA.
[Warren, Joseph D.; Urmy, Samuel S.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Southampton, NY USA.
[Sadro, Steven] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
[Chandra, Sudeep] Univ Nevada, Dept Biol, Reno, NV 89557 USA.
[Neale, Patrick J.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
RP Williamson, CE (reprint author), Miami Univ, Dept Biol, Oxford, OH 45056 USA.
EM craig.williamson@miamiOH.edu
FU NSF-DEB [1360066]
FX We thank B Allen, K Webb, and the staff of the UC Davis Tahoe
Environmental Research Center for critical assistance in the field at
Lake Tahoe, and the Blooming Grove Club for access to Lake Giles. This
work was supported by NSF-DEB #1360066.
NR 36
TC 3
Z9 3
U1 5
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1540-9295
EI 1540-9309
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD MAR
PY 2016
VL 14
IS 2
BP 102
EP 109
DI 10.1002/fee.1228
PG 8
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA DF7EJ
UT WOS:000371520300019
ER
PT J
AU Slater, GJ
Cui, P
Forasiepi, AM
Lenz, D
Tsangaras, K
Voirin, B
de Moraes-Barros, N
MacPhee, RDE
Greenwood, AD
AF Slater, Graham J.
Cui, Pin
Forasiepi, Analia M.
Lenz, Dorina
Tsangaras, Kyriakos
Voirin, Bryson
de Moraes-Barros, Nadia
MacPhee, Ross D. E.
Greenwood, Alex D.
TI Evolutionary Relationships among Extinct and Extant Sloths: The Evidence
of Mitogenomes and Retroviruses
SO GENOME BIOLOGY AND EVOLUTION
LA English
DT Article
DE sloth; mitogenomes; foamy virus; retrovirus-host coevolution; ancient
DNA; hybridization capture
ID GROUND SLOTH; PHYLOGENETIC-RELATIONSHIPS; FOAMY VIRUSES; ENDOGENOUS
RETROVIRUSES; PARTITIONING SCHEMES; MOLECULAR PHYLOGENY; MEGALONYCHID
SLOTH; MYLODON-DARWINII; SEQUENCE DATA; XENARTHRA
AB Macroevolutionary trends exhibited by retroviruses are complex and not entirely understood. The sloth endogenized foamy-like retrovirus (SloEFV), which demonstrates incongruence in virus-host evolution among extant sloths (Order Folivora), has not been investigated heretofore in any extinct sloth lineages and its premodern history within folivorans is therefore unknown. Determining retroviral coevolutionary trends requires a robust phylogeny of the viral host, but the highly reduced modern sloth fauna (6 species in 2 genera) does not adequately represent what was once a highly diversified clade (similar to 100 genera) of placental mammals. At present, the amount of molecular data available for extinct sloth taxa is limited, and analytical results based on these data tend to conflict with phylogenetic inferences made on the basis of morphological studies. To augment the molecular data set, we applied hybridization capture and next-generation Illumina sequencing to two extinct and three extant sloth species to retrieve full mitochondrial genomes (mitogenomes) from the hosts and the polymerase gene of SloEFV. The results produced a fully resolved and well-supported phylogeny that supports dividing crown families into two major clades: 1) The three-toed sloth, Bradypus, and Nothrotheriidae and 2) Megalonychidae, including the two-toed sloth, Choloepus, and Mylodontidae. Our calibrated time tree indicates that the Miocene epoch (23.5 Ma), particularly its earlier part, was an important interval for folivoran diversification. Both extant and extinct sloths demonstrate multiple complex invasions of SloEFV into the ancestral sloth germline followed by subsequent introgressions across different sloth lineages. Thus, sloth mitogenome and SloEFV evolution occurred separately and in parallel among sloths.
C1 [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
[Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA.
[Slater, Graham J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Cui, Pin; Lenz, Dorina; Tsangaras, Kyriakos; Greenwood, Alex D.] Leibniz Inst Zoo & Wildlife Res, Berlin, Germany.
[Forasiepi, Analia M.] IANIGLA, CCT Mendoza, Mendoza, Argentina.
[Voirin, Bryson] Max Planck Inst Ornithol, Seewiesen, Germany.
[de Moraes-Barros, Nadia] Univ Porto, Cibio Inbio Ctr Invest Biodiversidade & Recursos, Vairao, Portugal.
[MacPhee, Ross D. E.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA.
[MacPhee, Ross D. E.] Amer Museum Nat Hist, Div Vertebrate Zool, New York, NY 10024 USA.
[Greenwood, Alex D.] Free Univ Berlin, Dept Vet Med, Berlin, Germany.
RP Greenwood, AD (reprint author), Leibniz Inst Zoo & Wildlife Res, Berlin, Germany.; MacPhee, RDE (reprint author), Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA.; MacPhee, RDE (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool, New York, NY 10024 USA.; Greenwood, AD (reprint author), Free Univ Berlin, Dept Vet Med, Berlin, Germany.
EM macphee@amnh.org; greenwood@izw-berlin.de
FU National Institute of General Medical Sciences [R01GM092706]; China
Scholarship Council; Peter Buck postdoctoral fellowship through National
Museum of Natural History
FX The authors wish to thank Karin Honig and Susan Mbedi for excellent
technical assistance. The authors also thank Jochen Singer and Knut
Reinert for helpful discussions at the beginning of this project. The
authors wish to thank Alvaro Mones for helpful discussions on the
nomenclature of Octodontotherium grande. A.D.G. was supported by Grant
Number R01GM092706 from the National Institute of General Medical
Sciences. P.C. was supported by a fellowship from the China Scholarship
Council. G.J.S. was supported by a Peter Buck postdoctoral fellowship
through the National Museum of Natural History. The funders had no role
in study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 98
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U1 13
U2 20
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1759-6653
J9 GENOME BIOL EVOL
JI Genome Biol. Evol.
PD MAR
PY 2016
VL 8
IS 3
BP 607
EP 621
DI 10.1093/gbe/evw023
PG 15
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA DI9RD
UT WOS:000373839200013
PM 26878870
ER
PT J
AU Zong, JC
Heaggans, SY
Long, SY
Latimer, EM
Nofs, SA
Bronson, E
Casares, M
Fouraker, MD
Pearson, VR
Richman, LK
Hayward, GS
AF Zong, Jian-Chao
Heaggans, Sarah Y.
Long, Simon Y.
Latimer, Erin M.
Nofs, Sally A.
Bronson, Ellen
Casares, Miguel
Fouraker, Michael D.
Pearson, Virginia R.
Richman, Laura K.
Hayward, Gary S.
TI Detection of Quiescent Infections with Multiple Elephant
Endotheliotropic Herpesviruses (EEHVs), Including EEHV2, EEHV3, EEHV6,
and EEHV7, within Lymphoid Lung Nodules or Lung and Spleen Tissue
Samples from Five Asymptomatic Adult African Elephants
SO JOURNAL OF VIROLOGY
LA English
DT Article
ID CAPTIVE ASIAN ELEPHANTS; NEWLY RECOGNIZED DISEASE; HEMORRHAGIC-DISEASE;
MAXIMUS; VARIANTS; PCR
AB More than 80 cases of lethal hemorrhagic disease associated with elephant endotheliotropic herpesviruses (EEHVs) have been identified in young Asian elephants worldwide. Diagnostic PCR tests detected six types of EEHV in blood of elephants with acute disease, although EEHV1A is the predominant pathogenic type. Previously, the presence of herpesvirus virions within benign lung and skin nodules from healthy African elephants led to suggestions that African elephants may be the source of EEHV disease in Asian elephants. Here, we used direct PCR-basedDNAsequencing to detect EEHV genomes in necropsy tissue from five healthy adult African elephants. Two large lung nodules collected from culled wild South African elephants contained high levels of either EEHV3 alone or both EEHV2 and EEHV3. Similarly, a euthanized U.S. elephant proved to harbor multiple EEHV types distributed nonuniformly across four small lung nodules, including high levels of EEHV6, lower levels of EEHV3 and EEHV2, and a new GC-rich branch type, EEHV7. Several of the same EEHV types were also detected in random lung and spleen samples from two other elephants. Sanger PCR DNA sequence data comprising 100 kb were obtained from a total of 15 different strains identified, with (except for a few hypervariable genes) the EEHV2, EEHV3, and EEHV6 strains all being closely related to known genotypes from cases of acute disease, whereas the seven loci (4.0 kb) obtained from EEHV7 averaged 18% divergence from their nearest relative, EEHV3. Overall, we conclude that these four EEHV species, but probably not EEHV1, occur commonly as quiescent infections in African elephants.
C1 [Zong, Jian-Chao; Heaggans, Sarah Y.; Long, Simon Y.; Hayward, Gary S.] Johns Hopkins Sch Med, Viral Oncol Program, Bunting Blaustein Canc Res Bldg, Baltimore, MD USA.
[Latimer, Erin M.; Richman, Laura K.] Smithsonian Natl Zoo, Natl Elephant Herpesvirus Lab, Washington, DC USA.
[Nofs, Sally A.] Nashville Zoo Grassmere, Nashville, TN USA.
[Bronson, Ellen] Maryland Zoo Baltimore, Baltimore, MD USA.
[Casares, Miguel] Bioparc Valencia, Valencia, Spain.
[Fouraker, Michael D.] Ft Worth Zool Pk, Ft Worth, TX USA.
[Pearson, Virginia R.] Princeton Univ, Dept Mol Biol, Princeton, NJ 08544 USA.
[Nofs, Sally A.] Potter Pk Zoo, Lansing, MI USA.
[Pearson, Virginia R.] Fox Chase Canc Ctr, Rall Lab, 7701 Burholme Ave, Philadelphia, PA 19111 USA.
RP Hayward, GS (reprint author), Johns Hopkins Sch Med, Viral Oncol Program, Bunting Blaustein Canc Res Bldg, Baltimore, MD USA.
EM ghayward@jhmi.edu
FU Smithsonian Institution; Morris Animal Fund; Fort Worth Zoo;
International Elephant Foundation; Ringling Bros.; Barnum and Bailey
Center for Elephant Conservation; NIH [R01 AI24576]; Morris Animal
Foundation; Institute of Museums and Library Services
FX Studies at the Smithsonian National Zoo in Washington, DC, were funded
by Research grants to L.K.R. from the Smithsonian Institution, the
Morris Animal Fund, the Fort Worth Zoo, the International Elephant
Foundation, and Ringling Bros. and Barnum and Bailey Center for Elephant
Conservation. Studies at Johns Hopkins School of Medicine were funded
through NIH research grant R01 AI24576 to G.S.H., by a grant from the
Morris Animal Foundation in association with Fort Worth Zoo and the
International Elephant Foundation, and by a subcontract within a
Collections Stewardship Leadership grant from the Institute of Museums
and Library Services to Lauren Howard at the Houston Zoo in Texas.
NR 37
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U1 1
U2 3
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0022-538X
EI 1098-5514
J9 J VIROL
JI J. Virol.
PD MAR
PY 2016
VL 90
IS 6
BP 3028
EP 3043
DI 10.1128/JVI.02936-15
PG 16
WC Virology
SC Virology
GA DJ3MW
UT WOS:000374110600028
PM 26719245
ER
PT J
AU Kennedy, BRC
Quattrini, AM
Cheadle, MJ
Garcia-Moliner, G
Chaytor, J
Ford, M
Lobecker, M
Sowers, D
McKenna, L
Cantwell, K
Schmidt, W
Jimenez, M
Demopoulos, AWJ
Shank, TM
Scharer-Umpierre, M
Mah, CL
AF Kennedy, Brian R. C.
Quattrini, Andrea M.
Cheadle, Michael J.
Garcia-Moliner, Graciela
Chaytor, Jason
Ford, Michael
Lobecker, Meme
Sowers, Derek
McKenna, Lindsay
Cantwell, Kasey
Schmidt, Wilford
Jimenez, Manuel
Demopoulos, Amanda W. J.
Shank, Timothy M.
Scharer-Umpierre, Michelle
Mah, Christopher L.
CA Okeanos Explorer Onshore Sci Team
TI Oceano Profundo 2015: Exploring Puerto Rico's Seamounts, Trenches, and
Troughs
SO OCEANOGRAPHY
LA English
DT Editorial Material
C1 [Kennedy, Brian R. C.] NOAA, Off Ocean Explorat & Res, Narragansett, RI USA.
[Quattrini, Andrea M.] Harvey Mudd Coll, Southeast Ecol Sci Ctr, US Geol Survey, Claremont, CA 91711 USA.
[Cheadle, Michael J.] Univ Wyoming, Geol, Laramie, WY 82071 USA.
[Garcia-Moliner, Graciela] Caribbean Fishery Management Council, San Juan, PR USA.
[Chaytor, Jason] US Geol Survey, Woods Hole Coastal & Marine Sci Ctr, Woods Hole, MA 02543 USA.
[Ford, Michael; Cantwell, Kasey] NOAA, Natl Marine Fisheries Serv, Silver Spring, MD USA.
[Lobecker, Meme; Sowers, Derek; McKenna, Lindsay] NOAA, Off Ocean Explorat & Res, Durham, NH USA.
[Schmidt, Wilford] Univ Puerto Rico, Mayaguez, PR USA.
[Jimenez, Manuel] Univ Puerto Rico, Elect & Comp Engn, Mayaguez, PR USA.
[Jimenez, Manuel] Univ Puerto Rico, Dept Engn, Mayaguez, PR USA.
[Demopoulos, Amanda W. J.] US Geol Survey, Gainesville, FL USA.
[Shank, Timothy M.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Scharer-Umpierre, Michelle] Univ Puerto Rico, Interdisciplinary Ctr Coastal Studies, Mayaguez, PR USA.
[Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Kennedy, BRC (reprint author), NOAA, Off Ocean Explorat & Res, Narragansett, RI USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2016
VL 29
IS 1
SU S
BP 64
EP 67
PG 4
WC Oceanography
SC Oceanography
GA DJ3IM
UT WOS:000374098100019
ER
PT J
AU McManus, KM
Asner, GP
Martin, RE
Dexter, KG
Kress, WJ
Field, CB
AF McManus, Kelly M.
Asner, Gregory P.
Martin, Roberta E.
Dexter, Kyle G.
Kress, W. John
Field, Christopher B.
TI Phylogenetic Structure of Foliar Spectral Traits in Tropical Forest
Canopies
SO REMOTE SENSING
LA English
DT Article
DE functional traits; spectranomics; soil fertility; imaging spectroscopy;
phylogeny; phylogenetic signal; tropical forest; hyperspectral
ID BARRO COLORADO ISLAND; AMAZONIAN FOREST; HYPERSPECTRAL DISCRIMINATION;
FUNCTIONAL TRAITS; TRADE-OFF; COMMUNITY; LEAF; TREE; EVOLUTION; NITROGEN
AB The Spectranomics approach to tropical forest remote sensing has established a link between foliar reflectance spectra and the phylogenetic composition of tropical canopy tree communities vis-a-vis the taxonomic organization of biochemical trait variation. However, a direct relationship between phylogenetic affiliation and foliar reflectance spectra of species has not been established. We sought to develop this relationship by quantifying the extent to which underlying patterns of phylogenetic structure drive interspecific variation among foliar reflectance spectra within three Neotropical canopy tree communities with varying levels of soil fertility. We interpreted the resulting spectral patterns of phylogenetic signal in the context of foliar biochemical traits that may contribute to the spectral-phylogenetic link. We utilized a multi-model ensemble to elucidate trait-spectral relationships, and quantified phylogenetic signal for spectral wavelengths and traits using Pagel's lambda statistic. Foliar reflectance spectra showed evidence of phylogenetic influence primarily within the visible and shortwave infrared spectral regions. These regions were also selected by the multi-model ensemble as those most important to the quantitative prediction of several foliar biochemical traits. Patterns of phylogenetic organization of spectra and traits varied across sites and with soil fertility, indicative of the complex interactions between the environmental and phylogenetic controls underlying patterns of biodiversity.
C1 [McManus, Kelly M.; Asner, Gregory P.; Martin, Roberta E.; Field, Christopher B.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[McManus, Kelly M.; Asner, Gregory P.; Field, Christopher B.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Dexter, Kyle G.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3FF, Midlothian, Scotland.
[Dexter, Kyle G.] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland.
[Kress, W. John] Smithsonian Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA.
RP McManus, KM (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.; McManus, KM (reprint author), Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
EM mcmanusk@stanford.edu; gpa@carnegiescience.edu;
rmartin@carnegiescience.edu; kyle.dexter@ed.ac.uk; kressj@si.edu;
cfield@carnegiescience.edu
FU John D. and Catherine T. MacArthur Foundation
FX We thank the Spectranomics team for field, laboratory, and remote
sensing assistance. We thank Caroline Puente and the Smithsonian
Tropical Research Institute for assistance with the molecular data for
species collected at BCI, Panama, and we thank the Canadian Centre for
DNA Barcoding (CCDB) at the Biodiversity Institute of Ontario,
University of Guelph for assistance with the processing of genetic
sequences from sites in Tambopata, Peru. This study and the
Spectranomics Project are supported by the John D. and Catherine T.
MacArthur Foundation.
NR 69
TC 1
Z9 1
U1 8
U2 17
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAR
PY 2016
VL 8
IS 3
DI 10.3390/rs8030196
PG 16
WC Remote Sensing
SC Remote Sensing
GA DI6RJ
UT WOS:000373627400102
ER
PT J
AU Krech, S
AF Krech, Shepard, III
TI Life Beside Itself: Imagining Care in the Canadian Arctic
SO AMERICAN ANTHROPOLOGIST
LA English
DT Book Review
C1 [Krech, Shepard, III] Brown Univ, Providence, RI 02912 USA.
[Krech, Shepard, III] Smithsonian Inst, Washington, DC 20560 USA.
RP Krech, S (reprint author), Brown Univ, Providence, RI 02912 USA.; Krech, S (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7294
EI 1548-1433
J9 AM ANTHROPOL
JI Am. Anthropol.
PD MAR
PY 2016
VL 118
IS 1
BP 218
EP 219
DI 10.1111/aman.12490
PG 2
WC Anthropology
SC Anthropology
GA DI4TK
UT WOS:000373492000070
ER
PT J
AU Power, ML
AF Power, M. L.
TI Great ape milk differs from human milk in nutritionally significant ways
SO AMERICAN JOURNAL OF HUMAN BIOLOGY
LA English
DT Meeting Abstract
C1 [Power, M. L.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr,Nutr Lab, Washington, DC 20008 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1042-0533
EI 1520-6300
J9 AM J HUM BIOL
JI Am. J. Hum. Biol.
PD MAR-APR
PY 2016
VL 28
IS 2
BP 292
EP 292
PG 1
WC Anthropology; Biology
SC Anthropology; Life Sciences & Biomedicine - Other Topics
GA DH9RN
UT WOS:000373133500092
ER
PT J
AU Girard, JN
Zarka, P
Tasse, C
Hess, S
de Paters, I
Santos-Costa, D
Nenon, Q
Sicard, A
Bourdarie, S
Anderson, J
Asgekar, A
Bell, ME
van Bemmel, I
Bentum, MJ
Bernardi, G
Best, P
Bonafede, A
Breitling, F
Breton, RP
Broderick, JW
Brouw, WN
Bruggen, M
Ciardi, B
Corbel, S
Corstanje, A
de Gasperin, F
de Geus, E
Deller, A
Duscha, S
Eisloffel, J
Falcke, H
Frieswijk, W
Garrett, MA
Griessmeier, J
Gunst, AW
Hessels, JWT
Hoeft, M
Horandel, J
Iacobelli, M
Juette, E
Kondratiev, VI
Kuniyoshi, M
Kuper, G
van Leeuwen, J
Loose, M
Maat, P
Mann, G
Markoff, S
McFadden, R
McKay-Bukowski, D
Moldon, J
Munk, H
Nelles, A
Norden, MJ
Orru, E
Paas, H
Pandey-Pommier, M
Pizzo, R
Polatidis, AG
Reich, W
Roettgering, H
Rowlinson, A
Schwarz, D
Smirnov, O
Steinmetz, M
Swinbank, J
Tagger, M
Thoudam, S
Toribio, MC
Vermeulen, R
Vocks, C
van Weeren, RJ
Wijers, RAMJ
Wucknitz, O
AF Girard, J. N.
Zarka, P.
Tasse, C.
Hess, S.
de Paters, I.
Santos-Costa, D.
Nenon, Q.
Sicard, A.
Bourdarie, S.
Anderson, J.
Asgekar, A.
Bell, M. E.
van Bemmel, I.
Bentum, M. J.
Bernardi, G.
Best, P.
Bonafede, A.
Breitling, F.
Breton, R. P.
Broderick, J. W.
Brouw, W. N.
Brueggen, M.
Ciardi, B.
Corbel, S.
Corstanje, A.
de Gasperin, F.
de Geus, E.
Deller, A.
Duscha, S.
Eisloffel, J.
Falcke, H.
Frieswijk, W.
Garrett, M. A.
Griessmeier, J.
Gunst, A. W.
Hessels, J. W. T.
Hoeft, M.
Horandel, J.
Iacobelli, M.
Juette, E.
Kondratiev, V. I.
Kuniyoshi, M.
Kuper, G.
van Leeuwen, J.
Loose, M.
Maat, P.
Mann, G.
Markoff, S.
McFadden, R.
McKay-Bukowski, D.
Moldon, J.
Munk, H.
Nelles, A.
Norden, M. J.
Orru, E.
Paas, H.
Pandey-Pommier, M.
Pizzo, R.
Polatidis, A. G.
Reich, W.
Roettgering, H.
Rowlinson, A.
Schwarz, D.
Smirnov, O.
Steinmetz, M.
Swinbank, J.
Tagger, M.
Thoudam, S.
Toribio, M. C.
Vermeulen, R.
Vocks, C.
van Weeren, R. J.
Wijers, R. A. M. J.
Wucknitz, O.
TI Imaging Jupiter's radiation belts down to 127 MHz with LOFAR
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: magnetic fields; radio continuum: planetary
systems; techniques: interferometric
ID SYNCHROTRON-RADIATION; VLA OBSERVATIONS; MAGNETIC-FIELD; 3-DIMENSIONAL
RECONSTRUCTION; 3-D RECONSTRUCTION; RADIO-EMISSION; 22 CM; GHZ; MODELS;
ARRAY
AB Context. With the limited amount of in situ particle data available for the innermost region of Jupiter's magnetosphere, Earth-based observations of the giant planets synchrotron emission remain the sole method today of scrutinizing the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet. Radio observations ultimately provide key information about the origin and control parameters of the harsh radiation environment.
Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR. At a frequency as low as 127 MHz, the radiation from electrons with energies of similar to 1-30 MeV are expected, for the first time, to be measured and mapped over a broad region of Jupiter's inner magnetosphere.
Methods. Measurements consist of interferometric visibilities taken during a single 10-hour rotation of the Jovian system. These visibilities were processed in a custom pipeline developed for planetary observations, combining flagging, calibration, wide-field imaging, direction-dependent calibration, and specific visibility correction for planetary targets. We produced spectral image cubes of Jupiter's radiation belts at the various angular, temporal, and spectral resolutions from which flux densities were measured.
Results. The first resolved images of Jupiter's radiation belts at 127-172 MHz are obtained with a noise level similar to 20-25 mJy/beam, along with total integrated flux densities. They are compared with previous observations at higher frequencies. A greater extent of the synchrotron emission source (>= 4 R-J) is measured in the LOFAR range, which is the signature - as at higher frequencies - of the superposition of a "pancake" and an isotropic electron distribution. Asymmetry of east-west emission peaks is measured, as well as the longitudinal dependence of the radial distance of the belts, and the presence of a hot spot at lambda(III) = 230 degrees +/- 25 degrees. Spectral flux density measurements are on the low side of previous (unresolved) ones, suggesting a low-frequency turnover and/or time variations of the Jovian synchrotron spectrum.
Conclusions. LOFAR proves to be a powerful and flexible planetary imager. In the case of Jupiter, observations at 127 MHz depict the distribution of similar to 1-30 MeV energy electrons up to similar to 4-5 planetary radii. The similarities of the observations at 127 MHz with those at higher frequencies reinforce the conclusion that the magnetic field morphology primarily shapes the brightness distribution features of Jupiter's synchrotron emission, as well as how the radiating electrons are likely radially and latitudinally distributed inside about 2 planetary radii. Nonetheless, the detection of an emission region that extends to larger distances than at higher frequencies, combined with the overall lower flux density, yields new information on Jupiter's electron distribution, and this information may ultimately shed light on the origin and mode of transport of these particles.
C1 [Girard, J. N.; Corbel, S.] CEA Saclay, AIM, UMR, CEA CNRS Paris 7,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France.
[Tasse, C.] Observ Paris, CNRS, GEPI, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Hess, S.; Nenon, Q.; Sicard, A.; Bourdarie, S.] DESP, ONERA, 2 Av Edouard Belin, F-31055 Toulouse, France.
[de Paters, I.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA.
[Santos-Costa, D.] SW Res Inst, San Antonio, TX USA.
[Anderson, J.] Deutsch GeoForsch Zentrum GFZ, HelmholtzZentrum Potsdam, Dept Geodesy & Remote Sensing 1, Telegrafenberg A17, D-14473 Potsdam, Germany.
[Asgekar, A.; van Bemmel, I.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; Deller, A.; Duscha, S.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hessels, J. W. T.; Iacobelli, M.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Loose, M.; Maat, P.; McFadden, R.; Moldon, J.; Munk, H.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Rowlinson, A.; Vermeulen, R.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Asgekar, A.] Shell Technol Ctr, Bangalore, Karnataka, India.
[Bell, M. E.] CSIRO Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia.
[van Bemmel, I.] Joint Inst VLBI Europe, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands.
[Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Best, P.] Royal Observ, Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Breton, R. P.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Broderick, J. W.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Brouw, W. N.] Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Corstanje, A.; Falcke, H.; Horandel, J.; Nelles, A.; Thoudam, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[de Geus, E.] SmarterVision BV, Oostersingel 5, NL-9401 JX Assen, Netherlands.
[Eisloffel, J.; Hoeft, M.] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany.
[Garrett, M. A.; Roettgering, H.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Griessmeier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45100 Orleans, France.
[Griessmeier, J.] Univ Orleans, OSUC, CNRS INSU, USR 704,Observ Paris,Stn Radioastron Nancay, Route Souesmes, F-18330 Nancy, France.
[Hessels, J. W. T.; van Leeuwen, J.; Markoff, S.; Rowlinson, A.; Swinbank, J.; Wijers, R. A. M. J.] Univ Amsterdam, Anton Pannekoek Inst, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Juette, E.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany.
[Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Profsoyuznaya Str 84-32, Moscow 117997, Russia.
[Kuniyoshi, M.] Natl Astron Observ Japan, 2 Chome 21-1 Osawa, Mitaka, Tokyo, Japan.
[McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, Sodankyla 99600, Finland.
[McKay-Bukowski, D.] Rutherford Appleton Lab, STFC, Harwell Sci & Innovation Campus, Didcot OX11 0QX, Oxon, England.
[Paas, H.] Univ Groningen, CIT, NL-9712 CP Groningen, Netherlands.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Av Charles Andre, F-69561 St Genis Laval, France.
[Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Schwarz, D.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany.
[Girard, J. N.; Smirnov, O.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Girard, J. N.; Smirnov, O.] SKA South Africa, Park Rd, ZA-7405 Pinelands, South Africa.
[Toribio, M. C.] Leiden Univ, Leiden Observ, ALMA Reg Ctr, NL-2300 RA Leiden, Netherlands.
RP Girard, JN (reprint author), CEA Saclay, AIM, UMR, CEA CNRS Paris 7,Serv Astrophys, F-91191 Gif Sur Yvette, France.; Girard, JN (reprint author), Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.; Girard, JN (reprint author), SKA South Africa, Park Rd, ZA-7405 Pinelands, South Africa.
EM jgirard@ska.ac.za
RI Kondratiev, Vladislav/N-1105-2015; Breton, Rene/A-5536-2017;
OI Kondratiev, Vladislav/0000-0001-8864-7471; Breton,
Rene/0000-0001-8522-4983; Wijers, Ralph/0000-0002-3101-1808; Deller,
Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660
FU UnivEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023,
ANR-11-IDEX-0005-02]; European Research Council grant SparseAstro
[ERC-228261]
FX We acknowledge the financial support from the UnivEarthS Labex program
of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02) and
from the European Research Council grant SparseAstro (ERC-228261).
LOFAR, the Low Frequency Array designed and constructed by ASTRON, has
facilities in several countries that are owned by various parties (each
with their own funding sources) and that are collectively operated by
the International LOFAR Telescope (ILT) foundation under a joint
scientific policy. The authors thank Roberto Pizzo (ASTRON, Dwingeloo)
and Jean-Mathias Griessmeier (LPC2E, Orleans) for their assistance with
the observations, and thank James M. Anderson (co-author) for a thorough
final inspection of typos and notation convention.
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JI Astron. Astrophys.
PD MAR
PY 2016
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DI 10.1051/0004-6361/201527518
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800014
ER
PT J
AU Herpin, F
Chavarria, L
Jacq, T
Braine, J
van der Tak, F
Wyrowski, F
van Dishoeck, EF
Baudry, A
Bontemps, S
Kristensen, L
Schmalzl, M
Mata, J
AF Herpin, F.
Chavarria, L.
Jacq, T.
Braine, J.
van der Tak, F.
Wyrowski, F.
van Dishoeck, E. F.
Baudry, A.
Bontemps, S.
Kristensen, L.
Schmalzl, M.
Mata, J.
TI Herschel-HIFI view of mid-IR quiet massive protostellar objects
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; ISM: abundances; stars: formation; stars: protostars;
stars: early-type; line: profiles
ID STAR-FORMING REGIONS; H-II REGIONS; YOUNG STELLAR OBJECTS; NGC 6334 I;
MILLIMETER CONTINUUM; WATER ABUNDANCE; DENSE CORES; AFGL 2591;
CIRCUMSTELLAR ENVIRONMENT; INTERSTELLAR-MEDIUM
AB Aims. We present Herschel/MEI observations of 14 water lines in a small sample of Galactic massive protostellar objects: NGC 6334I(N), DR21(OH), IRAS 16272-4837, and IRAS 05358+3543. Using water as a tracer of the structure and kinematics, we individually study each of these objects with the aim to estimate the amount of water around them, but to also to shed light on the high-mass star formation process.
Methods. We analyzed the gas dynamics from the line profiles using Herschel-HIFI observations acquired as part of the WISH key project of 14 far-IR water lines ((H2O)-O-16, (H2O)-O-17, (H2O)-O-18) and several other species. Then through modeling the observations using the RATRAN radiative transfer code, we estimated outflow, infall, turbulent velocities, and molecular abundances and investigated the correlation with the evolutionary status of each source.
Results. The four sources (and the previously studied W43-MM1) have been ordered in terms of evolution based on their spectral energy distribution from youngest to older: 1) NGC 64334I(N); 2) W43-MM1; 3) DR21(011); 4) IRAS 16272-4837; 5) IRAS 05358+3543. The molecular line profiles exhibit a broad component coming from the shocks along the cavity walls that is associated with the protostars, and an infalling (or expanding, for IRAS 05358+3543) and passively heated envelope component, with highly supersonic turbulence that probably increases with the distance from the center. Accretion rates between 6.3 x 10(-5) and 5.6 x 10(-4) M-circle dot yr(-1) are derived from the infall observed in three of our sources. The outer water abundance is estimated to he at the typical value of a few 10(-8), while the inner abundance varies from 1.7 x 10(-6) to 1.4 x 10(-4) with respect to H-2 depending on the source.
Conclusions. We confirm that regions of massive star formation are highly turbulent and that the turbulence probably increases in the envelope with the distance to the star. The inner abundances are lower than the expected, 10(-4), perhaps because our observed lines do not probe deep enough into the inner envelope or because photodissociation through protostellar UV photons is more efficient than expected. We show that the higher the infall or expansion velocity in the protostellar envelope, the higher the inner abundance. This may indicate that higher infall or expansion velocities generate shocks that will sputter water from the ice mantles of dust grains in the inner region. High-velocity water must be formed in the gas phase from shocked material.
C1 [Herpin, F.; Chavarria, L.; Jacq, T.; Braine, J.; Baudry, A.; Bontemps, S.; Mata, J.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France.
[Herpin, F.; Chavarria, L.; Jacq, T.; Braine, J.; Baudry, A.; Bontemps, S.] CNRS, LAB, UMR 5804, F-33270 Floirac, France.
[Chavarria, L.] Univ Chile, CONICYT, Camino Observ 1515, Santiago, Chile.
[van der Tak, F.] SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands.
[Wyrowski, F.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[van Dishoeck, E. F.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Kristensen, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Herpin, F (reprint author), Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France.; Herpin, F (reprint author), CNRS, LAB, UMR 5804, F-33270 Floirac, France.
EM herpin@obs.u-bordeaux1.fr
RI Kristensen, Lars/F-4774-2011
OI Kristensen, Lars/0000-0003-1159-3721
FU Netherlands Research School for Astronomy (NOVA); Netherlands
Organisation for Scientific Research (NWO) [614.001.008]; European
Community's Seventh Framework Program FP7 [238258]; French Space Agency
CNES
FX This program was made possible thanks to the HIFI guaranteed time. HIFI
has been designed and built by a consortium of institutes and university
departments from across Europe, Canada and the United States under the
leadership of SRON Netherlands Institute for Space Research, Groningen,
The Netherlands and with major contributions from Germany, France and
the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR,
LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth;
Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF;
Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio
Astronomic Nacional (IGN), Centro de Astrobiologi (CSIC-INTA). Sweden:
Chalmers University of Technology - MC2; RSS & GARD; Onsala Space
Observatory; Swedish National Space Board, Stockholm University -
Stockholm Observatory; Switzerland: ETH Zurich, EHNW; USA: Caltech, JPL,
NHSC. HIPE is a joint development by the Herschel Science Ground Segment
Consortium, consisting of ESA, the NASA Herschel Science Center, and the
HIFI, PACS and SPIRE consortia. Astrochemistry in Leiden is supported by
the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant
and grant 614.001.008 from the Netherlands Organisation for Scientific
Research (NWO), and by the European Community's Seventh Framework
Program FP7/2007-2013 under grant agreement 238258 (LASSIE). We also
thank the French Space Agency CNES for financial support. We thank J.
Mottram for useful comments and discussions.
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PD MAR
PY 2016
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SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800150
ER
PT J
AU Lanza, AF
Molaro, P
Monaco, L
Haywood, RD
AF Lanza, A. F.
Molaro, P.
Monaco, L.
Haywood, R. D.
TI Long-term radial-velocity variations of the Sun as a star: The HARPS
view
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: radial velocities; planets and satellites: detection; Sun:
activity; Sun: magnetic fields; stars: activity
ID STELLAR ACTIVITY; PLANETARY SYSTEM; TIME-SERIES; IMPACT; GRANULATION;
SUNLIGHT; COROT-7; ATLAS
AB Context. Stellar radial velocities play a fundamental role in the discovery of extrasolar planets and the measurement of their physical parameters as well as in the study of stellar physical properties.
Aims. We investigate the impact of the solar activity on the radial velocity of the Sun using the HARPS spectrograph to obtain measurements that can be directly compared with those acquired in the extrasolar planet search programmes. Methods. We used the Moon, the Galilean satellites, and several asteroids as reflectors to measure the radial velocity of the Sun as a star and correlated this velocity with disc-integrated chromospheric and magnetic indexes of solar activity that are similar to stellar activity indexes. We discuss in detail the systematic effects that affect our measurements and the methods to account for them.
Results. We find that the radial velocity of the Sun as a star is positively correlated with the level of its chromospheric activity at similar to 95 percent significance level. The amplitude of the long-term variation measured in the 2006-2014 period is 4.98 +/- 1.44 m/s, which is in good agreement with model predictions. The standard deviation of the residuals obtained by subtracting a linear best fit is 2.82 m/s and is due to the rotation of the reflecting bodies and the intrinsic variability of the Sun on timescales shorter than the activity cycle. A correlation with a lower significance is detected between the radial velocity and the mean absolute value of the line-of-sight photospheric magnetic field flux density.
Conclusions. Our results confirm similar correlations found in other late-type main-sequence stars and provide support to the predictions of radial velocity variations induced by stellar activity based on current models.
C1 [Lanza, A. F.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy.
[Molaro, P.] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy.
[Monaco, L.] Univ Andres Bello, Dept Ciencias Fis, Republ 220, Santiago, Chile.
[Haywood, R. D.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Haywood, R. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Lanza, AF (reprint author), INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy.; Molaro, P (reprint author), INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy.; Monaco, L (reprint author), Univ Andres Bello, Dept Ciencias Fis, Republ 220, Santiago, Chile.; Haywood, RD (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.; Haywood, RD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nuccio.lanza@oact.inaf.it; molaro@oats.inaf.it; lorenzo.monaco@unab.cl;
rdh4@st-andrews.ac.uk
OI Lanza, Antonino Francesco/0000-0001-5928-7251
FU National Institute for Astrophysics (INAF); STFC studentship grant
[ST/J500744/1]; John Templeton Foundation
FX The authors are grateful to an anonymous referee for several valuable
comments and suggestions that helped them to improve their work. They
wish to thank Prof. Andrew Collier Cameron and Dr. Christophe Lovis for
interesting discussions. AFL acknowledges support from the National
Institute for Astrophysics (INAF) through the Progetti premiali funding
scheme of the Italian Ministry of Education, University and Research.
RDH was supported by STFC studentship grant ST/J500744/1 during the
course of this work. R.D.H. gratefully acknowledges a grant from the
John Templeton Foundation. The opinions expressed in this publication
are those of the authors and do not necessarily reflect the views of the
John Templeton Foundation. This work utilizes Ca II K solar data
obtained at Sacramento Peak Observatory and SOLIS data obtained by the
NSO Integrated Synoptic Program (NISP), managed by the National Solar
Observatory, which is operated by the Association of Universities for
Research in Astronomy (AURA), Inc. under a cooperative agreement with
the National Science Foundation. The authors also gratefully acknowledge
the availability of HARPS data obtained from the ESO Science Archive
Facility and the use of JPL NASA Horizons Ephemerides.
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JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A103
DI 10.1051/0004-6361/201527379
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800114
ER
PT J
AU Lasota, JP
Vieira, RSS
Sadowski, A
Narayan, R
Abramowicz, MA
AF Lasota, J. -P.
Vieira, R. S. S.
Sadowski, A.
Narayan, R.
Abramowicz, M. A.
TI The slimming effect of advection on black-hole accretion flows
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; black hole physics
ID RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS; SUPER-EDDINGTON ACCRETION;
X-RAY SOURCES; DOMINATED ACCRETION; THICK ACCRETION; VERTICAL STRUCTURE;
POLISH DOUGHNUTS; TIDAL DISRUPTION; DISK MODEL; JETS
AB Context. At super-Eddington rates accretion flows onto black holes have been described as slim (aspect ratio H/R less than or similar to 1) or thick (H/R > 1) discs, also known as tori or (Polish) doughnuts. The relation between the two descriptions has never been established, but it was commonly believed that at sufficiently high accretion rates slim discs inflate, becoming thick.
Aims. We wish to establish under what conditions slim accretion flows become thick.
Methods. We use analytical equations, numerical 1 + 1 schemes, and numerical radiative MHD codes to describe and compare various accretion flow models at very high accretion rates.
Results. We find that the dominant effect of advection at high accretion rates precludes slim discs becoming thick.
Conclusions. At super-Eddington rates accretion flows around black holes can always be considered slim rather than thick.
C1 [Lasota, J. -P.] CNRS, Inst Astrophys Paris, 98Bis Bd Arago, F-75014 Paris, France.
[Lasota, J. -P.] Univ Paris 06, Sorbonne Univ, UMR 7095, 98Bis Bd Arago, F-75014 Paris, France.
[Lasota, J. -P.; Vieira, R. S. S.; Abramowicz, M. A.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
[Vieira, R. S. S.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil.
[Sadowski, A.] MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Narayan, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Abramowicz, M. A.] Gothenburg Univ, Dept Phys, S-41296 Gothenburg, Sweden.
RP Lasota, JP (reprint author), CNRS, Inst Astrophys Paris, 98Bis Bd Arago, F-75014 Paris, France.; Lasota, JP (reprint author), Univ Paris 06, Sorbonne Univ, UMR 7095, 98Bis Bd Arago, F-75014 Paris, France.; Lasota, JP (reprint author), Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
EM lasota@iap.fr
OI Narayan, Ramesh/0000-0002-1919-2730; Vieira, Ronaldo/0000-0002-0995-1385
FU Polish NCN grant [UMO-2013/08/A/ST9/00795, DEC-2012/04/A/ST9/00083];
French Space Agency CNES; Fundacao de Amparo a Pesquisa do Estado de Sao
Paulo (FAPESP) [2010/00487-9, 2013/01001-0, 2015/10577-9]; NASA through
Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF4-150126];
NASA [NAS8-03060]; NSF via XSEDE resources [TG-AST080026N]
FX We are grateful to Wlodek Kluzniak for helpful comments. We thank Maciek
Wielgus for his help with PDs and Fig. 6. The anonymous referee's report
was very helpful. This research was supported by the Polish NCN grants
UMO-2013/08/A/ST9/00795 and DEC-2012/04/A/ST9/00083. J.P.L. was
supported in part by a grant from the French Space Agency CNES. R.S.S.V.
was supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo
(FAPESP), grants 2010/00487-9, 2013/01001-0 and 2015/10577-9. R.S.S.V.
is grateful for the hospitality at Harvard-Smithsonian Center for
Astrophysics and at Nicolaus Copernicus Astronomical Center. A.S.
acknowledges support for this work by NASA through Einstein Postdoctoral
Fellowship number PF4-150126 awarded by the Chandra X-ray Center, which
is operated by the Smithsonian Astrophysical Observatory for NASA under
contract NAS8-03060. A.S. acknowledges computational support from NSF
via XSEDE resources (grant TG-AST080026N), and from NASA via the
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
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JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A13
DI 10.1051/0004-6361/201527636
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800024
ER
PT J
AU Meingast, S
Alves, J
Mardones, D
Teixeira, PS
Lombardi, M
Grossschedl, J
Ascenso, J
Bouy, H
Forbrich, J
Goodman, A
Hacar, A
Hasenberger, B
Kainulainen, J
Kubiak, K
Lada, C
Lada, E
Moitinho, A
Petr-Gotzens, M
Rodrigues, L
Roman-Zuniga, CG
AF Meingast, Stefan
Alves, Joao
Mardones, Diego
Teixeira, Paula Stella
Lombardi, Marco
Grossschedl, Josefa
Ascenso, Joana
Bouy, Herve
Forbrich, Jan
Goodman, Alyssa
Hacar, Alvaro
Hasenberger, Birgit
Kainulainen, Jouni
Kubiak, Karolina
Lada, Charles
Lada, Elizabeth
Moitinho, Andre
Petr-Gotzens, Monika
Rodrigues, Lara
Roman-Zuniga, Carlos G.
TI VISION - Vienna survey in Orion I. VISTA Orion A Survey
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: image processing; methods: data analysis; stars: formation;
stars: pre-main sequence
ID FIELD EXTINCTION MAPS; YOUNG STELLAR OBJECTS; MOLECULAR CLOUD COMPLEX;
NEBULA-CLUSTER; STAR-FORMATION; PROPER MOTIONS; IMAGING SURVEY; SKY
SURVEY; ASTRONOMICAL IMAGES; MONOCEROS R2
AB Context. Orion A hosts the nearest massive star factory, thus offering a unique opportunity to resolve the processes connected with the formation of both low- and high-mass stars. Here we present the most detailed and sensitive near-infrared (NIR) observations of the entire molecular cloud to date.
Aims. With the unique combination of high image quality, survey coverage, and sensitivity, our NIR survey of Orion A aims at establishing a solid empirical foundation for further studies of this important cloud. In this first paper we present the observations, data reduction, and source catalog generation. To demonstrate the data quality, we present a first application of our catalog to estimate the number of stars currently forming inside Orion A and to verify the existence of a more evolved young foreground population.
Methods. We used the European Southern Observatory's (ESO) Visible and Infrared Survey Telescope for Astronomy (VISTA) to survey the entire Orion A molecular cloud in the NIR J, H, and K-S bands, covering a total of similar to 18.3 deg(2). We implemented all data reduction recipes independently of the ESO pipeline. Estimates of the young populations toward Orion A are derived via the K-S-band luminosity function.
Results. Our catalog (799 995 sources) increases the source counts compared to the Two Micron All Sky Survey by about an order of magnitude. The 90% completeness limits are 20.4, 19.9, and 19.0 mag in J, H, and K-S, respectively. The reduced images have 20% better resolution on average compared to pipeline products. We find between 2300 and 3000 embedded objects in Orion A and confirm that there is an extended foreground population above the Galactic field, in agreement with previous work.
Conclusions. The Orion A VISTA catalog represents the most detailed NIR view of the nearest massive star-forming region and provides a fundamental basis for future studies of star formation processes toward Orion.
C1 [Meingast, Stefan; Alves, Joao; Teixeira, Paula Stella; Grossschedl, Josefa; Forbrich, Jan; Hacar, Alvaro; Hasenberger, Birgit; Kubiak, Karolina] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Mardones, Diego; Rodrigues, Lara] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile.
[Lombardi, Marco] Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy.
[Ascenso, Joana] Univ Lisbon, Inst Super Tecn, CENTRA, Ave Rovisco Pais 1, P-1049001 Lisbon, Portugal.
[Ascenso, Joana] Univ Porto, Dept Engn Fis, Fac Engn, Rua Dr Roberto Frias S-N, P-4200465 Oporto, Portugal.
[Bouy, Herve] CSIC, Ctr Astrobiol, INTA, Dept Astrofis, POB 78, Madrid 28691, Spain.
[Forbrich, Jan; Goodman, Alyssa; Lada, Charles] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kainulainen, Jouni] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Lada, Elizabeth] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Moitinho, Andre] Univ Lisbon, Fac Ciencias, SIM CENTRA, Ed C8, P-1749016 Lisbon, Portugal.
[Petr-Gotzens, Monika] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Roman-Zuniga, Carlos G.] UNAM, Inst Astron, Ensenada 22860, Baja California, Mexico.
RP Meingast, S (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM stefan.meingast@univie.ac.at
RI Bouy, Herve/H-2913-2012; Teixeira, Paula Stella/O-2289-2013;
OI Moitinho de Almeida, Andre/0000-0003-0822-5995; Bouy,
Herve/0000-0002-7084-487X; Teixeira, Paula Stella/0000-0002-3665-5784;
Hacar, Alvaro/0000-0001-5397-6961; LOMBARDI, MARCO/0000-0002-3336-4965;
Goodman, Alyssa/0000-0003-1312-0477; Meingast,
Stefan/0000-0002-0568-5526
FU Austrian Academy of Sciences at the Institute for Astrophysics,
University of Vienna; Austrian Science Fund (FWF) [P 26718-N27]; NASA
[NCC5-626]; California Institute of Technology [NCC5-626]; Ramon y Cajal
fellowship [RYC-2009-04497]; [AYA2012-38897-C02-01]
FX Stefan Meingast is a recipient of a DOC Fellowship of the Austrian
Academy of Sciences at the Institute for Astrophysics, University of
Vienna. This work has been supported by the Austrian Science Fund (FWF)
under project number P 26718-N27. We gratefully acknowledge the referee,
Tom Megeath, for carefully reading the manuscript and the useful
comments that served to improve both the clarity and quality of this
study. This research made use of Montage, funded by the National
Aeronautics and Space Administration's Earth Science Technology Office,
Computation Technologies Project, under Cooperative Agreement Number
NCC5-626 between NASA and the California Institute of Technology.
Montage is maintained by the NASA/IPAC Infrared Science Archive; The
SIMBAD database, operated at the CDS, Strasbourg, France. "Aladin sky
atlas" developed at the CDS, Strasbourg Observatory, France. The VizieR
catalogue access tool, CDS, Strasbourg, France. Astropy is a
community-developed core Python package for Astronomy (Astropy
Collaboration et al. 2013). H. Bouy is supported by the Ramon y Cajal
fellowship program number RYC-2009-04497 and by the Spanish Grant
AYA2012-38897-C02-01.
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PY 2016
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SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800164
ER
PT J
AU Schneider, N
Bontemps, S
Motte, F
Ossenkopf, V
Klessen, RS
Simon, R
Fechtenbaum, S
Herpin, F
Tremblin, P
Csengeri, T
Myers, PC
Hill, T
Cunningham, M
Federrath, C
AF Schneider, N.
Bontemps, S.
Motte, F.
Ossenkopf, V.
Klessen, R. S.
Simon, R.
Fechtenbaum, S.
Herpin, F.
Tremblin, P.
Csengeri, T.
Myers, P. C.
Hill, T.
Cunningham, M.
Federrath, C.
TI Understanding star formation in molecular clouds III. Probability
distribution functions of molecular lines in Cygnus X
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: abundances; ISM: clouds; dust, extinction; ISM: molecules; ISM:
structure
ID TURBULENT MAGNETIZED CLOUDS; LARGE-SCALE STRUCTURE; COLUMN DENSITY;
HERSCHEL VIEW; DARK CLOUDS; INTERSTELLAR CLOUDS; MASSIVE STARS; CO;
REGION; COMPLEX
AB The probability distribution function of column density (N-PDF) serves as a powerful tool to characterise the various physical processes that influence the structure of molecular clouds. Studies that use extinction maps or H-2 column-density maps (N) that are derived from dust show that star-forming clouds can best be characterised by lognormal PDFs for the lower N range and a power-law tail for higher N, which is commonly attributed to turbulence and self-gravity and/or pressure, respectively. While PDFs from dust cover a large dynamic range (typically N similar to 10(20-24) cm(-2) or A(v) similar to 0.1-1000), PDFs obtained from molecular lines -converted into H-2 column density - potentially trace more selectively different regimes of (column) densities and temperatures. They also enable us to distinguish different clouds along the line of sight through using the velocity information. We report here on PDFs that were obtained from observations of (CO)-C-12, (CO)-C-13, (CO)-O-18, CS, and N2H+ in the Cygnus X North region, and make a comparison to a PDF that was derived from dust observations with the Herschel satellite. The PDF of (CO)-C-12 is lognormal for A(v) similar to 1-30, but is cut for higher Av because of optical depth effects. The PDFs of (CO)-O-18 and (CO)-C-13 are mostly lognormal up to A(v) similar to 1-15, followed by excess up to A(v) similar to 40. Above that value, all CO PDFs drop, which is most likely due to depletion. The high density tracers CS and N2H+ exhibit only a power law distribution between A(v) similar to 15 and 400, respectively. The PDF from dust is lognormal for A(v) similar to 3-15 and has a power-law tail up to A(v) similar to 500. Absolute values for the molecular line column densities are, however, rather uncertain because of abundance and excitation temperature variations. If we take the dust PDF at face value, we "calibrate" the molecular line PDF of CS to that of the dust and determine an abundance [CS]/[H-2] of 10(-9). The slopes of the power-law tails of the CS, N2H+, and dust PDFs are -1.6, -1.4, and -2.3, respectively, and are thus consistent with free-fall collapse of filaments and clumps. A quasi static configuration of filaments and clumps can also possibly account for the observed N-PDFs, providing they have a sufficiently condensed density structure and external ram pressure by gas accretion is provided. The somehow flatter slopes of N2H+ and CS can reflect an abundance change and/or subthermal excitation at low column densities.
C1 [Schneider, N.; Bontemps, S.; Fechtenbaum, S.; Herpin, F.] Univ Bordeaux, CNRS, LAB, UMR 5804, F-33270 Floirac, France.
[Schneider, N.; Ossenkopf, V.; Simon, R.] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
[Motte, F.] Univ Paris Diderot, Lab AIM CNRS, IRFU SAp CEA DSM, F-91191 Gif Sur Yvette, France.
[Klessen, R. S.] Heidelberg Univ, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
[Tremblin, P.] CEA Saclay, Maison Simulat, F-91191 Gif Sur Yvette, France.
[Csengeri, T.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Myers, P. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Hill, T.] Joint ALMA Observ, Santiago 15782, Chile.
[Cunningham, M.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Federrath, C.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
RP Schneider, N (reprint author), Univ Bordeaux, CNRS, LAB, UMR 5804, F-33270 Floirac, France.; Schneider, N (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
EM nschneid@ph1.uni-koeln.de
OI Tremblin, Pascal/0000-0001-6172-3403; Cunningham,
Maria/0000-0001-7020-6176
FU project STARFICH [ANR-11-BS56-010]; Deutsche Forschungsgemeinschaft, DFG
[0s 177/2-1, 177/2-2]; DFG-priority program [1573]; Australian Research
Councils Discovery Projects [DP130102078, DP150104329]; DFG priority
program [1573]; collaborative research project [SFB 881]
FX N.S. and S.B. acknowledge support by the ANR-11-BS56-010 project
STARFICH. N.S., V.O., and T.C. acknowledge support from the Deutsche
Forschungsgemeinschaft, DFG, through project number 0s 177/2-1 and
177/2-2, and central funds of the DFG-priority program 1573 (ISM-SPP).
C.F. acknowledges funding provided by the Australian Research Councils
Discovery Projects (grants DP130102078 and DP150104329). R.S.K.
acknowledges subsidies from the DFG priority program 1573 (Physics of
the Interstellar Medium) and the collaborative research project SFB 881
(The Milky Way System, subprojects B1, B2, and B5).
NR 86
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A74
DI 10.1051/0004-6361/201527144
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800085
ER
PT J
AU Starkenburg, TK
Helmi, A
Sales, LV
AF Starkenburg, T. K.
Helmi, A.
Sales, L. V.
TI Dark influences II. Gas and star formation in minor mergers of dwarf
galaxies with dark satellites
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: interactions; galaxies:
irregular; galaxies: starburst; dark matter
ID LOW-MASS GALAXIES; MATTER HALOES; LOCAL VOLUME; H I; FORMATION
HISTORIES; FORMATION RATES; COSMOLOGICAL SIMULATIONS;
INTERSTELLAR-MEDIUM; IRREGULAR GALAXIES; SUPERNOVA FEEDBACK
AB Context. It has been proposed that mergers induce starbursts and lead to important morphological changes in galaxies. Most studies so far have focused on large galaxies, but dwarfs might also experience such events, since the halo mass function is scale-free in the concordance cosmological model. Notably, because of their low mass, most of their interactions will be with dark satellites.
Aims. In this paper we follow the evolution of gas-rich disky dwarf galaxies as they experience a minor merger with a dark satellite. We aim to characterize the effects of such an interaction on the dwarf's star formation, morphology, and kinematical properties.
Methods. We performed a suite of carefully set-up hydrodynamical simulations of dwarf galaxies that include dark matter, gas, and stars merging with a satellite consisting solely of dark matter. For the host system we vary the gas fraction, disk size and thickness, halo mass, and concentration, while we explore different masses, concentrations, and orbits for the satellite.
Results. We find that the interactions cause strong starbursts of both short and long duration in the dwarfs. Their star formation rates increase by factors of a few to 10 or more. They are strongest for systems with extended gas disks and high gas fractions merging with a high-concentration satellite on a planar, radial orbit. In contrast to analogous simulations of Milky Way-mass galaxies, many of the systems experience strong morphological changes and become spheroidal even in the presence of significant amounts of gas.
Conclusions. The simulated systems compare remarkably well with the observational properties of a large selection of irregular dwarf galaxies and blue compact dwarfs. This implies that mergers with dark satellites might well be happening but not be fully evident, and may thus play a role in the diversity of the dwarf galaxy population.
C1 [Starkenburg, T. K.; Helmi, A.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Sales, L. V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Sales, L. V.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
RP Starkenburg, TK (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
EM tjitske@astro.rug.nl
FU European Research Council under ERC-StG grant [GALACTICA-240271];
Netherlands Research Organisation NWO
FX We are grateful to Claudio Dalla Vecchia, Joop Schaye, Carlos Vera-Ciro,
Alvaro Villalobos and Volker Springel for providing code. AH
acknowledges financial support from the European Research Council under
ERC-StG grant GALACTICA-240271 and the Netherlands Research Organisation
NWO for a Vici grant.
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A24
DI 10.1051/0004-6361/201527247
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800035
ER
PT J
AU Sudar, D
Saar, SH
Skokic, I
Beljan, IP
Brajsa, R
AF Sudar, D.
Saar, S. H.
Skokic, I.
Beljan, I. Poljancic
Brajsa, R.
TI Meridional motions and Reynolds stress from SDO/AIA coronal bright
points data
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: rotation; Sun: corona; Sun: activity
ID SOLAR DIFFERENTIAL ROTATION; SOHO-EIT IMAGES; RECURRENT SUNSPOT GROUPS;
TORSIONAL OSCILLATIONS; AUTOMATIC METHODS; CONVECTION ZONE;
MOUNT-WILSON; SUN; CIRCULATION; VELOCITY
AB Context. It is possible to detect and track coronal bright points (CBPs) in Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) images. A combination of high resolution and high cadence provides a wealth of data that can be used to determine velocity flows on the solar surface with very high accuracy.
Aims. We derived a very accurate solar rotation profile and investigated meridional flows, torsional oscillations, and horizontal Reynolds stress based on approximate to 6 months of SDO/AIA data.
Methods. We used a segmentation algorithm to detect CBPs in SDO/AIA images. We also used invariance of the solar rotation profile with central meridian distance (CMD) to determine the height of CBPs in the 19.3 nm channel.
Results. The best fit solar rotation profile is given by omega(b) = (14.4060 +/- 0.0051 + (-1.662 +/- 0.050) sin(2) b + (-2.742 +/- 0.081) sin(4) b)degrees day(-1). The height of CBPs in the SDO/AIA 19.3 nm channel was found to be approximate to 6500 km. Meridional motion is predominantly poleward for all latitudes, while solar velocity residuals show signs of torsional oscillations. Horizontal Reynolds stress was found to be smaller than in similar works, but still showed transfer of angular momentum towards the solar equator.
Conclusions. Most of the results are consistent with Doppler measurements rather than tracer measurements. The fairly small calculated value of horizontal Reynolds stress might be due to the particular phase of the solar cycle. Accuracy of the calculated rotation profile indicates that it is possible to measure changes in the profile as the solar cycle evolves. Analysis of further SDO/AIA CBP data will also provide a better understanding of the temporal behaviour of the rotation velocity residuals, meridional motions, and Reynolds stress.
C1 [Sudar, D.; Brajsa, R.] Univ Zagreb, Fac Geodesy, Hvar Observ, Kaciceva 26, Zagreb 10000, Croatia.
[Saar, S. H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Skokic, I.] Acad Sci Czech Republic, Inst Astron, Fricova 298, CS-25165 Ondrejov, Czech Republic.
[Beljan, I. Poljancic] Univ Rijeka, Dept Phys, Radmile Matejcic 2, Rijeka 51000, Croatia.
RP Sudar, D (reprint author), Univ Zagreb, Fac Geodesy, Hvar Observ, Kaciceva 26, Zagreb 10000, Croatia.
EM davor.sudar@gmail.com
FU Croatian Science Foundation [6212]; SOLARNET project [312495]; FP7
Capacities Programme [I3]; NASA [NNX09AB03G]; Lockheed-Martin
[SP02H1701R]
FX This work has been supported in part by the Croatian Science Foundation
under the project 6212 "Solar and Stellar Variability". It has also
received funding from the SOLARNET project (312495, 2013-2017), which is
an Integrated Infrastructure Initiative (I3) supported by FP7 Capacities
Programme. S.S. was supported by NASA Grant NNX09AB03G to the
Smithsonian Astrophysical Observatory and contract SP02H1701R from
Lockheed-Martin to SAO.
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A29
DI 10.1051/0004-6361/201527217
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800040
ER
PT J
AU van Kempen, TA
Hogerheijde, MR
van Dishoeck, EF
Kristensen, LE
Belloche, A
Klaassen, PD
Leurini, S
San Jose-Garcia, I
Aykutalp, A
Choi, Y
Endo, A
Frieswijk, W
Harsono, D
Karska, A
Koumpia, E
van der Marel, N
Nagy, Z
Perez-Beaupuits, JP
Risacher, C
van Weeren, RJ
Wyrowski, F
Yildiz, UA
Gusten, R
Boland, W
Baryshev, A
AF van Kempen, T. A.
Hogerheijde, M. R.
van Dishoeck, E. F.
Kristensen, L. E.
Belloche, A.
Klaassen, P. D.
Leurini, S.
San Jose-Garcia, I.
Aykutalp, A.
Choi, Y.
Endo, A.
Frieswijk, W.
Harsono, D.
Karska, A.
Koumpia, E.
van der Marel, N.
Nagy, Z.
Perez-Beaupuits, J. -P.
Risacher, C.
van Weeren, R. J.
Wyrowski, F.
Yildiz, U. A.
Guesten, R.
Boland, W.
Baryshev, A.
TI Outflow forces in intermediate-mass star formation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; stars: formation; ISM: jets and outflows;
submillimeter: ISM
ID YOUNG STELLAR OBJECTS; HIGH-J CO; HERSCHEL-PACS SPECTROSCOPY; PROTOSTAR
SERPENS SMM1; VELA MOLECULAR CLOUDS; JCMT LEGACY SURVEY; NGC-7129 FIRS
2; FORMING REGIONS; ENVELOPE STRUCTURE; CLASS-0 SOURCES
AB Context. Protostars of intermediate-mass provide a bridge between theories of low-and high-mass star formation. Molecular outflows emerging from such sources can be used to determine the influence of fragmentation and multiplicity on protostellar evolution through the apparent correlation of outflow forces of intermediate-mass protostars with the total luminosity instead of the individual luminosity.
Aims. The aim of this paper is to derive outflow forces from outflows of six intermediate-mass protostellar regions and validate the apparent correlation between total luminosity and outflow force seen in earlier work, as well as remove uncertainties caused by different methodologies.
Methods. By comparing CO 6-5 observations obtained with APEX with non-LTE radiative transfer model predictions, the optical depths, temperatures and densities of the gas of the molecular outflows are derived. Outflow forces, dynamical timescales, and kinetic luminosities are subsequently calculated.
Results. Outflow parameters, including the forces, were derived for all sources. Temperatures in excess of 50 K were found for all flows, in line with recent low-mass results. However, comparison with other studies could not corroborate conclusions from earlier work on intermediate-mass protostars which hypothesized that fragmentation enhances outflow forces in clustered intermediate-mass star formation. Any enhancement in comparison with the classical relation between outflow force and luminosity can be attributed to the use of a higher excitation line and improvement in methods. They are in line with results from low-mass protostars using similar techniques.
Conclusions. The role of fragmentation on outflows is an important ingredient to understand clustered star formation and the link between low- and high-mass star formation. However, detailed information on spatial scales of a few 100 AU, covering all individual members is needed to make the necessary progress.
C1 [van Kempen, T. A.; Hogerheijde, M. R.; van Dishoeck, E. F.; Kristensen, L. E.; Klaassen, P. D.; San Jose-Garcia, I.; Harsono, D.; Karska, A.; van der Marel, N.; van Weeren, R. J.; Yildiz, U. A.; Boland, W.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[van Kempen, T. A.] Joint ALMA Off, Ave Alonso Cordova 3107, Santiago, Chile.
[van Dishoeck, E. F.; Karska, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 2, D-85478 Garching, Germany.
[Kristensen, L. E.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Belloche, A.; Leurini, S.; Perez-Beaupuits, J. -P.; Risacher, C.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Klaassen, P. D.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aykutalp, A.; Choi, Y.; Koumpia, E.; Nagy, Z.; Baryshev, A.] Univ Groningen, Kapteyn Inst, Landleven 12, NL-9747 AD Groningen, Netherlands.
[Aykutalp, A.] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
[Choi, Y.; Koumpia, E.; Nagy, Z.; Risacher, C.; Baryshev, A.] SRON Netherlands Inst Space Res, Low Energy Astrophys Div, Postbus 800, NL-9700 AV Groningen, Netherlands.
[Endo, A.] Delft Univ Technol, Fac Elect Engn Math & Comp Sci, Dept Microelect, NL-2628 CD Delft, Netherlands.
[Endo, A.] Delft Univ Technol, Kavli Inst Nanosci, Dept Quantum Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands.
[Frieswijk, W.] Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Karska, A.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Sloneczna 36, PL-60286 Poznan, Poland.
[Yildiz, U. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Boland, W.] Netherlands Res Sch Astron, POB 9513, NL-2300 RA Leiden, Netherlands.
RP van Kempen, TA (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.; van Kempen, TA (reprint author), Joint ALMA Off, Ave Alonso Cordova 3107, Santiago, Chile.
EM kempen@strw.leidenuniv.nl
RI Kristensen, Lars/F-4774-2011; Yildiz, Umut/C-5257-2011; Karska,
Agata/O-5311-2016;
OI Kristensen, Lars/0000-0003-1159-3721; Yildiz, Umut/0000-0001-6197-2864;
Karska, Agata/0000-0001-8913-925X; Perez-Beaupuits,
Juan-Pablo/0000-0003-3536-2274; van Weeren, Reinout/0000-0002-0587-1660
FU Allegro ARC node in Leiden; NOVA (Nederlandse Onderzoeksschool voor
Astronomie); NWO (Nederlandse Organisatie voor Wetenschappelijk
Onderzoek); NASA through the Einstein Postdoctoral grant - Chandra X-ray
Center [PF2-130104]; NASA [NAS8-03060]; Polish National Science Center
grant [2013/11/N/ST9/00400]; Foundation for Polish Science (FNP);
Netherlands Organization for Scientific Research (NWO) [600.063.310.10]
FX T.v.K. is supported by the Allegro ARC node in Leiden and NOVA
(Nederlandse Onderzoeksschool voor Astronomie) and NWO (Nederlandse
Organisatie voor Wetenschappelijk Onderzoek). R.J.v.W. acknowledges
support provided by NASA through the Einstein Postdoctoral grant number
PF2-130104 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. A.K. acknowledges support from the Polish National Science
Center grant 2013/11/N/ST9/00400 and the Foundation for Polish Science
(FNP). Construction of CHAMP+ was a collaboration between the
Max-Planck-Institut fur Radioastronomie Bonn, Germany; SRON Netherlands
Institute for Space Research, Groningen, The Netherlands; The
Netherlands Research School for Astronomy (NOVA); and the Kavli
Institute of Nanoscience at Delft University of Technology, the
Netherlands; with support from the Netherlands Organization for
Scientific Research (NWO) grant 600.063.310.10. We thank the APEX staff,
in particular the scientists (Per Bergman, Andreas Lundgren, Michael
Dumke, Francisco Montenegro and Rodrigo Parra) and operators (Francisco
"Pancho" Azagra, Claudio Agurto, Felipe Mac Auliffe, Paulina Venegas and
Mauricio Martinez) for their warm welcome over the years.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A17
DI 10.1051/0004-6361/201424725
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800028
ER
PT J
AU Zari, E
Lombardi, M
Alves, J
Lada, CJ
Bouy, H
AF Zari, Eleonora
Lombardi, Marco
Alves, Joao
Lada, Charles J.
Bouy, Herve
TI Herschel-Planck dust optical depth and column density maps II. Perseus
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; dust, extinction; ISM: individual objects: Perseus
molecular could; methods: data analysis; ISM: structure
ID INFRARED-SURVEY-EXPLORER; NEARBY MOLECULAR CLOUDS; SMALL-SCALE
STRUCTURES; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; SPITZER C2D
SURVEY; SCHMIDT LAW; NGC 1333; EVOLUTION; CLUSTERS
AB We present optical depth and temperature maps of the Perseus molecular cloud, obtained combining dust emission data from the Herschel and Planck satellites and 2MASS/NIR dust extinction maps. The maps have a resolution of 36 arcsec in the Herschel regions, and of 5 arcmin elsewhere. The dynamic range of the optical depth map ranges from 1 x 10(-2) mag up to 20 mag in the equivalent K-band extinction. We also evaluate the ratio between the 2.2 mu m extinction coefficient and the 850 mu m opacity. The value we obtain is close to the one found in the Orion B molecular cloud. We show that the cumulative and the differential area function of the data ( which is proportional to the probability distribution function of the cloud column density) follow power laws with an index of respectively similar or equal to-2, and similar or equal to-3. We use WISE data to improve current YSO catalogs based mostly on Spitzer data and we build an up-to-date selection of Class I/0 objects. Using this selection, we evaluate the local Schmidt law, Sigma(YSO) proportional to Sigma(beta)(gas), showing that beta = 2.4 +/- 0.6. Finally, we show that the area-extinction relation is important for determining the star-formation rate in the cloud, which is in agreement with other recent works.
C1 [Zari, Eleonora] Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Zari, Eleonora; Lombardi, Marco] Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy.
[Alves, Joao] Univ Vienna, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Mail Stop 72,60 Garden St, Cambridge, MA 02138 USA.
[Bouy, Herve] Ctr Astrobiol, INTA CSIC, POB 78, Madrid 28691, Spain.
RP Zari, E (reprint author), Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.; Zari, E (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy.
EM zariem@strw.leidenuniv.nl
RI Bouy, Herve/H-2913-2012;
OI Bouy, Herve/0000-0002-7084-487X; LOMBARDI, MARCO/0000-0002-3336-4965;
Alves, Joao/0000-0002-4355-0921
FU National Aeronautics and Space Administration; ESA Member States, NASA;
ESA Member States, Canada; National Science Foundation
FX We thank the anonymous referee for comments that improved the
manuscript. We also wish to thank Josefa Grossscheld and Paula Stella
Teixeira for the helpful discussions. This publication would not have
been possible without the data products from the Herschel satellite and
the Wide-field Infrared Survey Explorer (WISE). Herschel is an ESA space
observatory with science instruments provided by European-led Principal
Investigator Consortia and with important participation from NASA. WISE
is a joint project of the University of California, Los Angeles, and the
Jet Propulsion Laboratory/California Institute of Technology, funded by
the National Aeronautics and Space Administration. This paper is also
based on observations obtained with Planck (http://www.esa.int/Planck),
an ESA science mission with instruments and contributions directly
funded by ESA Member States, NASA, and Canada. Furthermore, it makes use
of data products from the Two Micron All Sky Survey, which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation. This research made use of: the SIMBAD database, operated at
CDS, Strasbourg, France; the VizieR catalogue access tool, CDS,
Strasbourg, France: Astropy, a community developed core Python package
for Astronomy (Astropy Collaboration et al. 2013); TORCAT, an
interactive graphical viewer and editor for tabular data (Taylor 2005).
NR 52
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A106
DI 10.1051/0004-6361/201526597
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800117
ER
PT J
AU Fleming, CH
Fagan, WF
Mueller, T
Olson, KA
Leimgruber, P
Calabrese, JM
AF Fleming, C. H.
Fagan, W. F.
Mueller, T.
Olson, K. A.
Leimgruber, P.
Calabrese, J. M.
TI Estimating where and how animals travel: an optimal framework for path
reconstruction from autocorrelated tracking data
SO ECOLOGY
LA English
DT Article
DE autocorrelation; Brownian bridge; CRAWL; Krige; Mongolian gazelle;
Procapra gutturosa; telemetry error; tracking data; tracking data gaps;
utilization distribution
ID CORRELATED RANDOM-WALK; BROWNIAN-MOTION; TELEMETRY DATA; HOME-RANGE;
MOVEMENT; MODEL; INDEPENDENCE; SCALES; TIME
AB An animal's trajectory is a fundamental object of interest in movement ecology, as it directly informs a range of topics from resource selection to energy expenditure and behavioral states. Optimally inferring the mostly unobserved movement path and its dynamics from a limited sample of telemetry observations is a key unsolved problem, however. The field of geostatistics has focused significant attention on a mathematically analogous problem that has a statistically optimal solution coined after its inventor, Krige. Kriging revolutionized geostatistics and is now the gold standard for interpolating between a limited number of autocorrelated spatial point observations. Here we translate Kriging for use with animal movement data. Our Kriging formalism encompasses previous methods to estimate animal's trajectoriesthe Brownian bridge and continuous-time correlated random walk libraryas special cases, informs users as to when these previous methods are appropriate, and provides a more general method when they are not. We demonstrate the capabilities of Kriging on a case study with Mongolian gazelles where, compared to the Brownian bridge, Kriging with a more optimal model was 10% more precise in interpolating locations and 500% more precise in estimating occurrence areas.
C1 [Fleming, C. H.; Mueller, T.; Olson, K. A.; Leimgruber, P.; Calabrese, J. M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
[Fleming, C. H.; Fagan, W. F.; Mueller, T.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Mueller, T.] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr, Senckenberganlage 25, D-60325 Frankfurt, Germany.
[Mueller, T.] Goethe Univ Frankfurt, Dept Biol Sci, Max von Laue Str 9, D-60438 Frankfurt, Germany.
RP Fleming, CH (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.; Fleming, CH (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
EM FlemingC@si.edu
RI Calabrese, Justin/B-9131-2012; Leimgruber, Peter/O-1304-2015
OI Leimgruber, Peter/0000-0002-3682-0153
FU US National Science Foundation [ABI 1062411, ABI 1458748]; Smithsonian
Institution postdoctoral fellowship; Robert Bosch Foundation
FX The project was funded by US National Science Foundation grants ABI
1062411 and ABI 1458748. C. H. Fleming was funded by a Smithsonian
Institution postdoctoral fellowship. T. Mueller was funded by the Robert
Bosch Foundation.
NR 33
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD MAR
PY 2016
VL 97
IS 3
BP 576
EP 582
DI 10.1890/15-1607.1
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA DI5UL
UT WOS:000373565900004
PM 27197385
ER
PT J
AU Paudel, S
Longcore, T
MacDonald, B
McCormick, MK
Szlavecz, K
Wilson, GWT
Loss, SR
AF Paudel, Shishir
Longcore, Travis
MacDonald, Beau
McCormick, Melissa K.
Szlavecz, Katalin
Wilson, Gail W. T.
Loss, Scott R.
TI Belowground interactions with aboveground consequences: Invasive
earthworms and arbuscular mycorrhizal fungi
SO ECOLOGY
LA English
DT Article
DE arbuscular mycorrhizal fungi; disturbance; earthworm invasion; ecosystem
engineers; plant community; plant-soil interactions
ID NORTHERN HARDWOOD FORESTS; PLANT COMMUNITY STRUCTURE; TALLGRASS PRAIRIE;
NONNATIVE EARTHWORMS; INTRODUCED EARTHWORMS; BIOLOGICAL INVASIONS; SOIL
CHARACTERISTICS; NESTING SONGBIRDS; TEMPERATE FORESTS; EXOTIC EARTHWORMS
AB A mounting body of research suggests that invasive nonnative earthworms substantially alter microbial communities, including arbuscular mycorrhizal fungi (AMF). These changes to AMF can cascade to affect plant communities and vertebrate populations. Despite these research advances, relatively little is known about (1) the mechanisms behind earthworms' effects on AMF and (2) the factors that determine the outcomes of earthworm-AMF interactions (i.e., whether AMF abundance is increased or decreased and subsequent effects on plants). We predict that AMF-mediated effects of nonnative earthworms on ecosystems are nearly universal because (1) AMF are important components of most terrestrial ecosystems, (2) nonnative earthworms have become established in nearly every type of terrestrial ecosystem, and (3) nonnative earthworms, due to their burrowing and feeding behavior, greatly affect AMF with potentially profound concomitant effects on plant communities. We highlight the multiple direct and indirect effects of nonnative earthworms on plants and review what is currently known about the interaction between earthworms and AMF. We also illustrate how the effects of nonnative earthworms on plant-AMF mutualisms can alter the structure and stability of aboveground plant communities, as well as the vertebrate communities relying on these habitats. Integrative studies that assess the interactive effects of earthworms and AMF can provide new insights into the role that belowground ecosystem engineers play in altering aboveground ecological processes. Understanding these processes may improve our ability to predict the structure of plant and animal communities in earthworm-invaded regions and to develop management strategies that limit the numerous undesired impacts of earthworms.
C1 [Paudel, Shishir; Wilson, Gail W. T.; Loss, Scott R.] Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA.
[Longcore, Travis] Univ So Calif, Sch Architecture, Los Angeles, CA 90089 USA.
[Longcore, Travis] Univ So Calif, Spatial Sci Inst, Los Angeles, CA 90089 USA.
[Longcore, Travis; MacDonald, Beau] Urban Wildlands Grp, POB 24020, Los Angeles, CA 90024 USA.
[McCormick, Melissa K.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
[Szlavecz, Katalin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Paudel, S (reprint author), Oklahoma State Univ, Dept Nat Resource Ecol & Management, Stillwater, OK 74078 USA.
EM paudelshishir@gmail.com
RI Longcore, Travis/A-4978-2008
OI Longcore, Travis/0000-0002-1039-2613
FU U.S. Department of the Navy, Commander Pacific Fleet [W9126G-13-2-0047]
FX S. Paudel, T. Longcore, B. MacDonald, and S. R. Loss were funded by the
U.S. Department of the Navy, Commander Pacific Fleet, through
cooperative agreement number W9126G-13-2-0047. We thank David Gibson and
two anonymous reviewers for helpful comments on the manuscript.
NR 104
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD MAR
PY 2016
VL 97
IS 3
BP 605
EP 614
DI 10.1890/15-1085
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA DI5UL
UT WOS:000373565900007
PM 27197388
ER
PT J
AU Chen, YX
Wright, SJ
Muller-Landau, HC
Hubbell, SP
Wang, YF
Yu, SX
AF Chen, Yuxin
Wright, S. Joseph
Muller-Landau, Helene C.
Hubbell, Stephen P.
Wang, Yongfan
Yu, Shixiao
TI Positive effects of neighborhood complementarity on tree growth in a
Neotropical forest
SO ECOLOGY
LA English
DT Article
DE biodiversity and ecosystem functioning; complementarity;
individual-based method; neighborhood dissimilarity; phylogeny; plant
functional trait; productivity; shade tolerance
ID TROPICAL FOREST; DENSITY-DEPENDENCE; FUNCTIONAL TRAITS; SHADE TOLERANCE;
DIVERSITY; COMMUNITY; SEEDLINGS; BIODIVERSITY; RECRUITMENT; COMPETITION
AB Numerous grassland experiments have found evidence for a complementarity effect, an increase in productivity with higher plant species richness due to niche partitioning. However, empirical tests of complementarity in natural forests are rare. We conducted a spatially explicit analysis of 518433 growth records for 274 species from a 50-ha tropical forest plot to test neighborhood complementarity, the idea that a tree grows faster when it is surrounded by more dissimilar neighbors. We found evidence for complementarity: focal tree growth rates increased by 39.8% and 34.2% with a doubling of neighborhood multi-trait dissimilarity and phylogenetic dissimilarity, respectively. Dissimilarity from neighbors in maximum height had the most important effect on tree growth among the six traits examined, and indeed, its effect trended much larger than that of the multi-trait dissimilarity index. Neighborhood complementarity effects were strongest for light-demanding species, and decreased in importance with increasing shade tolerance of the focal individuals. Simulations demonstrated that the observed neighborhood complementarities were sufficient to produce positive stand-level biodiversity-productivity relationships. We conclude that neighborhood complementarity is important for productivity in this tropical forest, and that scaling down to individual-level processes can advance our understanding of the mechanisms underlying stand-level biodiversity-productivity relationships.
C1 [Chen, Yuxin; Wang, Yongfan; Yu, Shixiao] Sun Yat Sen Univ, Dept Ecol, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China.
[Wright, S. Joseph; Muller-Landau, Helene C.; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
RP Yu, SX (reprint author), Sun Yat Sen Univ, Dept Ecol, Sch Life Sci, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China.
EM lssysx@mail.sysu.edu.cn
RI Wright, Stuart/M-3311-2013
OI Wright, Stuart/0000-0003-4260-5676
FU National Natural Science Foundation of China [31230013, 31011120470];
Zhang-Hongda Science Foundation in SYSU; National Science Foundation of
the United States [DEB 1046113]; F. H. Levinson Fund; National Science
and MacArthur Foundations
FX We thank Fangliang He, Xinghua Sui, Chunchao Zhu, Jesse R. Lasky, and
anonymous referees for their helpful comments on the manuscript; Nadja
Ruger for help in coding to address measurement errors; and David L.
Erickson and Edwin Lebrija-Trejos for providing the phylogenetic tree.
This research was funded by the National Natural Science Foundation of
China (31230013 and 31011120470), the Zhang-Hongda Science Foundation in
SYSU, the National Science Foundation of the United States (DEB 1046113)
and the F. H. Levinson Fund. The BCI plot has been made possible through
the support of the National Science and MacArthur Foundations and
hundreds of people over the last three decades.
NR 45
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD MAR
PY 2016
VL 97
IS 3
BP 776
EP 785
DI 10.1890/15-0625.1
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA DI5UL
UT WOS:000373565900022
PM 27197403
ER
PT J
AU Ayres, TR
Kashyap, V
Saar, S
Huenemoerder, D
Korhonen, H
Drake, JJ
Testa, P
Cohen, O
Garraffo, C
Granzer, T
Strassmeier, K
AF Ayres, Thomas R.
Kashyap, V.
Saar, S.
Huenemoerder, D.
Korhonen, H.
Drake, J. J.
Testa, P.
Cohen, O.
Garraffo, C.
Granzer, T.
Strassmeier, K.
TI FK COMAE BERENICES, KING OF SPIN: THE COCOA-PUFS PROJECT
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars: coronae; stars: individual (HD 117555=FK Com); ultraviolet:
stars; X-rays: stars
ID TELESCOPE IMAGING SPECTROGRAPH; LOCAL INTERSTELLAR-MEDIUM; X-RAY; EK
DRACONIS; STARS; CORONA; MASS; MORPHOLOGY; SPECTRUM; CHANDRA
AB COCOA-PUFS is an energy-diverse, time-domain study of the ultra-fast spinning, heavily spotted, yellow giant FK Comae Berenices (FK Com: HD117555; G4 III). This single star is thought to be a recent binary merger, and is exceptionally active by measure of its intense ultraviolet (UV) and X-ray emissions, and proclivity to flare. COCOA-PUFS was carried out with the Hubble Space Telescope in the UV (1200-3000 angstrom), using mainly its high-performance Cosmic Origins Spectrograph, but also high precision Space Telescope Imaging Spectrograph; Chandra X-ray Observatory in the soft X-rays (0.5-10 keV), utilizing its High-Energy Transmission Grating Spectrometer; together with supporting photometry and spectropolarimetry in the visible from the ground. This is an introductory report on the project. FK Com displayed variability on a wide range of timescales over all wavelengths during the week-long main campaign, including a large X-ray flare; "super-rotational broadening" of the far-ultraviolet "hot lines" (e.g., Si IV 1393 angstrom; 8 x 10(4) K) together with chromospheric Mg II 2800 angstrom and C II 1335 angstrom (1-3. x. 10(4) K); large Doppler swings suggestive of bright regions alternately on advancing and retreating limbs of the star; and substantial redshifts of the epoch-average emission profiles. These behaviors paint a picture of a highly extended, dynamic, hot (similar to 10 MK) coronal magnetosphere around the star, threaded by cooler structures perhaps analogous to solar prominences and replenished continually by surface activity and flares. Suppression of angular momentum loss by the confining magnetosphere could temporarily postpone the inevitable stellar spindown, thereby lengthening this highly volatile stage of coronal evolution.
C1 [Ayres, Thomas R.] Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
[Kashyap, V.; Saar, S.; Drake, J. J.; Testa, P.; Cohen, O.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Huenemoerder, D.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Korhonen, H.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Granzer, T.; Strassmeier, K.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
RP Ayres, TR (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
EM Thomas.Ayres@Colorado.edu
RI Korhonen, Heidi/E-3065-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; Cohen, Ofer/0000-0003-3721-0215
FU Space Telescope Science Institute [GO-12279, GO-12376, GO-13938];
Smithsonian Astrophysical Observatory [GO1-12021X, GO1-12037X]; NASA
[NAS8-03060]; NASA through SAO [SV3-73016]; European Community's Seventh
Framework Program under (OPTICON) [RG226604]; ESO Telescopes at the La
Silla Paranal Observatory [087.D-0294]
FX This work was supported by grants GO-12279, GO-12376, and GO-13938 from
the Space Telescope Science Institute, based on observations from Hubble
Space Telescope collected at STScI, operated by the Associated
Universities for Research in Astronomy, under contract to NASA; and
grants GO1-12021X and GO1-12037X from the Smithsonian Astrophysical
Observatory, based on observations from the Chandra X-ray Observatory,
collected and processed at the Chandra X-ray Center, operated by SAO
under contract to NASA. V.K. and J.J.D. were supported by NASA contract
NAS8-03060 to the CXC. D.P.H. was supported by NASA through SAO contract
SV3-73016 to MIT for the CXC and Science Instruments. The research
leading to these results has received funding from the European
Community's Seventh Framework Program (FP7/2007-2013) under grant
agreement number RG226604 (OPTICON). Special thanks goes to the
schedulers of HST and Chandra, who were able to successfully carry out
the challenging coordination of the two space observatories during the
main campaign period in 2011 April. This project made use of public
databases hosted by SIMBAD, maintained by CDS, Strasbourg, France; the
Mikulski Archive for Space Telescopes at STScI in Baltimore, Maryland;
and the High Energy Astrophysics Science and Research Center at the NASA
Goddard Space Flight Center, in Greenbelt, Maryland. We also thank the
various ground-based facilities for their support of the FK. Com
campaign, including especially the ESO Telescopes at the La Silla
Paranal Observatory under program 087.D-0294.
NR 44
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2016
VL 223
IS 1
AR 5
DI 10.3847/0067-0049/223/1/5
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0TB
UT WOS:000373208900005
ER
PT J
AU Smillie, DG
Pickering, JC
Nave, G
Smith, PL
AF Smillie, D. G.
Pickering, J. C.
Nave, G.
Smith, P. L.
TI THE SPECTRUM AND TERM ANALYSIS OF CO III MEASURED USING FOURIER
TRANSFORM AND GRATING SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic data; line: identification; line: profiles; methods: laboratory:
atomic
ID DOUBLY IONIZED ATOMS; IRON-GROUP ELEMENTS; VACUUM-ULTRAVIOLET;
ENERGY-LEVELS; CONFIGURATIONS; WAVELENGTHS; 3RD; UV; SPECTROMETER;
MULTIPLET
AB The spectrum of Co III has been recorded in the region 1562-2564 angstrom (64,000 cm(-1)-39,000 cm(-1)) by Fourier transform (FT) spectroscopy, and in the region 1317-2500 angstrom (164,000 cm(-1)-40,000 cm(-1)) using a 10.7 m grating spectrograph with phosphor image plate detectors. The spectrum was excited in a cobalt-neon Penning discharge lamp. We classified 514 Co III lines measured using FT spectroscopy, the strongest having wavenumber uncertainties approaching 0.004 cm(-1) (approximately 0.2 m angstrom at 2000 angstrom, or 1 part in 10(7)), and 240 lines measured with grating spectroscopy with uncertainties between 5 and 10 m angstrom. The wavelength calibration of 790 lines of Raassen & Orti Ortin and 87 lines from Shenstone has been revised and combined with our measurements to optimize the values of all but one of the 288 previously reported energy levels. Order of magnitude reductions in uncertainty for almost two-thirds of the 3d(6)4s and almost half of the 3d(6)4p revised energy levels are obtained. Ritz wavelengths have been calculated for an additional 100 forbidden lines. Eigenvector percentage compositions for the energy levels and predicted oscillator strengths have been calculated using the Cowan code.
C1 [Smillie, D. G.; Pickering, J. C.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
[Nave, G.] NIST, Gaithersburg, MD 20899 USA.
[Smith, P. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Pickering, JC (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
EM j.pickering@imperial.ac.uk
FU NASA [NAG5-12668, W-10,255, NNH10AH38I]; STFC; PPARC (UK); Royal Society
of the UK; Leverhulme Trust
FX This work was supported in part by NASA grant NAG5-12668, NASA
inter-agency agreements W-10,255 and NNH10AH38I, the STFC and PPARC
(UK), the Royal Society of the UK, and by the Leverhulme Trust.
NR 50
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U1 3
U2 4
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2016
VL 223
IS 1
AR 12
DI 10.3847/0067-0049/223/1/12
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0TB
UT WOS:000373208900012
ER
PT J
AU van Weeren, RJ
Williams, WL
Hardcastle, MJ
Shimwell, TW
Rafferty, DA
Sabater, J
Heald, G
Sridhar, SS
Dijkema, TJ
Brunetti, G
Bruggen, M
Andrade-Santos, F
Ogrean, GA
Rottgering, HJA
Dawson, WA
Forman, WR
de Gasperin, F
Jones, C
Miley, UK
Rudnick, L
Sarazin, CL
Bonafede, A
Best, PN
Birzan, L
Cassano, R
Chyzy, KT
Croston, JH
Ensslin, T
Ferrari, C
Hoeft, M
Horellou, C
Jarvis, MJ
Kraft, RP
Mevius, M
Intema, HT
Murray, SS
Orru, E
Pizzo, R
Simionescu, A
Stroe, A
van der Tol, S
White, GJ
AF van Weeren, R. J.
Williams, W. L.
Hardcastle, M. J.
Shimwell, T. W.
Rafferty, D. A.
Sabater, J.
Heald, G.
Sridhar, S. S.
Dijkema, T. J.
Brunetti, G.
Brueggen, M.
Andrade-Santos, F.
Ogrean, G. A.
Roettgering, H. J. A.
Dawson, W. A.
Forman, W. R.
de Gasperin, F.
Jones, C.
Miley, U. K.
Rudnick, L.
Sarazin, C. L.
Bonafede, A.
Best, P. N.
Birzan, L.
Cassano, R.
Chyzy, K. T.
Croston, J. H.
Ensslin, T.
Ferrari, C.
Hoeft, M.
Horellou, C.
Jarvis, M. J.
Kraft, R. P.
Mevius, M.
Intema, H. T.
Murray, S. S.
Orru, E.
Pizzo, R.
Simionescu, A.
Stroe, A.
van der Tol, S.
White, G. J.
TI LOFAR FACET CALIBRATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE techniques: interferometric
ID RADIO INTERFEROMETRIC CALIBRATION; WIDE-FIELD; GAIN CALIBRATION;
SELF-CALIBRATION; W-PROJECTION; SKY SURVEY; ALGORITHM; I.; ASTRONOMY;
SYSTEM
AB LOFAR, the Low-Frequency Array, is a powerful new radio telescope operating between 10 and 240 MHz. LOFAR allows detailed sensitive high-resolution studies of the low-frequency radio sky. At the same time LOFAR also provides excellent short baseline coverage to map diffuse extended emission. However, producing highquality deep images is challenging due to the presence of direction-dependent calibration errors, caused by imperfect knowledge of the station beam shapes and the ionosphere. Furthermore, the large data volume and presence of station clock errors present additional difficulties. In this paper we present a new calibration scheme, which we name facet calibration, to obtain deep high-resolution LOFAR High Band Antenna images using the Dutch part of the array. This scheme solves and corrects the direction-dependent errors in a number of facets that cover the observed field of view. Facet calibration provides close to thermal noise limited images for a typical 8 hr observing run at similar to 5. resolution, meeting the specifications of the LOFAR Tier-1 northern survey.
C1 [van Weeren, R. J.; Andrade-Santos, F.; Ogrean, G. A.; Forman, W. R.; Jones, C.; Kraft, R. P.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Williams, W. L.; Shimwell, T. W.; Roettgering, H. J. A.; de Gasperin, F.; Miley, U. K.; Stroe, A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Williams, W. L.; Heald, G.; Sridhar, S. S.; Dijkema, T. J.; Mevius, M.; Orru, E.; Pizzo, R.; van der Tol, S.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Williams, W. L.; Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Rafferty, D. A.; Brueggen, M.; de Gasperin, F.; Bonafede, A.; Birzan, L.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Sabater, J.; Best, P. N.] Royal Observ, Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Heald, G.; Sridhar, S. S.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Brunetti, G.; Cassano, R.] INAF, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
[Dawson, W. A.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA.
[Rudnick, L.] Univ Minnesota, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Chyzy, K. T.] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Ensslin, T.] Max Planck Inst Astrophys, Karl Schwarzschildstr 1, D-85741 Garching, Germany.
[Ferrari, C.] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Hoeft, M.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
[Horellou, C.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Jarvis, M. J.] Oxford Astrophys, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
[Jarvis, M. J.] Univ Western Cape, ZA-7535 Bellville, South Africa.
[Intema, H. T.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA.
[Simionescu, A.] JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[White, G. J.] Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England.
RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rvanweeren@cfa.harvard.edu
RI Intema, Huib/D-1438-2012;
OI Intema, Huib/0000-0002-5880-2730; Seethapuram Sridhar,
Sarrvesh/0000-0002-7587-4779; Hardcastle, Martin/0000-0003-4223-1117;
Sabater, Jose/0000-0003-1149-6294; van Weeren,
Reinout/0000-0002-0587-1660
FU NASA through the Einstein Postdoctoral grant [PF2-130104]; NASA
[NAS8-03060, NAS5-26555]; National Aeronautics and Space Administration
through Chandra Award [GO3-14138X]; National Aeronautics Space
Administration [NAS8-03060]; NASA through a Hubble Fellowship - Space
Telescope Science Institute [HST-HF2-51345.001-A]; Alexander von
Humboldt Foundation; PRIN-INAF; Smithsonian Institution; Agence
Nationale pour la Recherche, MAGEL-LAN project [ANR-14-CE23-0004-01];
NSF [AST-1211595]; U.S. DOE by LLNL [DE-AC52-07NA27344]; [G03-14131X]
FX We would like to thank the anonymous referee for useful comments. R.J.W.
was supported by NASA through the Einstein Postdoctoral grant number
PF2-130104 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO3-14138X, issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060. G.A.O. acknowledges support by NASA through a Hubble
Fellowship grant HST-HF2-51345.001-A awarded by the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
G.B. acknowledges support from the Alexander von Humboldt Foundation. G.
B. and R.C. acknowledge support from PRIN-INAF 2014. W.R.F., C.J., and
F.A.-S. acknowledge support from the Smithsonian Institution. F.A.-S.
acknowledges support from Chandra grant G03-14131X. C.F. acknowledges
support by the Agence Nationale pour la Recherche, MAGEL-LAN project,
ANR-14-CE23-0004-01. Partial support for L.R. is provided by NSF Grant
AST-1211595 to the University of Minnesota. Part of this work performed
under the auspices of the U.S. DOE by LLNL under Contract
DE-AC52-07NA27344. LOFAR, the Low Frequency Array designed and
constructed by ASTRON, has facilities in several countries that are
owned by various parties (each with their own funding sources), and that
are collectively operated by the International LOFAR Telescope (ILT)
foundation under a joint scientific policy. We thank the staff of the
GMRT that made these observations possible. GMRT is run by the National
Centre for Radio Astrophysics of the Tata Institute of Fundamental
Research. The Open University is incorporated by Royal Charter (RC
000391), an exempt charity in England & Wales and a charity registered
in Scotland (SC 038302). The Open University is authorized and regulated
by the Financial Conduct Authority.
NR 45
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2016
VL 223
IS 1
AR 2
DI 10.3847/0067-0049/223/1/2
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0TB
UT WOS:000373208900002
ER
PT J
AU Lesoway, MP
AF Lesoway, Maryna P.
TI The future of Evo-Devo: the inaugural meeting of the Pan American
Society for evolutionary developmental biology
SO EVOLUTION & DEVELOPMENT
LA English
DT Article
ID SEPSIDAE DIPTERA; ANIMAL EMBRYOS; LEAF SHAPE; PLASTICITY; STICKLEBACKS;
MECHANISMS; SOLANACEAE; REVEALS; PATTERN; PATHWAY
AB What is the future of evolutionary developmental biology? This question and more were discussed at the inaugural meeting for the Pan American Society for Evolutionary Developmental Biology, held August 5-9, 2015, in Berkeley, California, USA. More than 300 participants attended the first meeting of the new society, representing the current diversity of Evo-Devo. Speakers came from throughout the Americas, presenting work using an impressive range of study systems, techniques, and approaches. Current research draws from themes including the role of gene regulatory networks, plasticity and the role of the environment, novelty, population genetics, and regeneration, using new and emerging techniques as well as traditional tools. Multiple workshops and a discussion session covered subjects both practical and theoretical, providing an opportunity for members to discuss the current challenges and future directions for Evo-Devo. The excitement and discussion generated over the course of the meeting demonstrates the current dynamism of the field, suggesting that the future of Evo-Devo is bright indeed.
C1 [Lesoway, Maryna P.] McGill Univ, Dept Biol, 1205 Ave Dr Penfield, Montreal, PQ H3A 1B1, Canada.
[Lesoway, Maryna P.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
RP Lesoway, MP (reprint author), McGill Univ, Dept Biol, 1205 Ave Dr Penfield, Montreal, PQ H3A 1B1, Canada.; Lesoway, MP (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
EM maryna.lesoway@mail.mcgill.ca
FU Quebec Centre for Biodiversity Science; NSERC
FX I thank the organizers of the meeting: Nipam Patel, Christopher Lowe,
Karen Sears, and especially Ehab Abouheif, who gave me the opportunity
to write this report. This manuscript is my own interpretation of the
presentations and discussions that took place in Berkeley, August 5-9,
2015. I thank all of the speakers for their excellent presentations,
particularly those whose work I have referenced here, and apologize to
those whose work was not included due to space limitations. Thank you to
the Quebec Centre for Biodiversity Science for an Excellence Award that
contributed to meeting costs and NSERC Discovery Grant to Ehab Abouheif
for funding.
NR 57
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1520-541X
EI 1525-142X
J9 EVOL DEV
JI Evol. Dev.
PD MAR-APR
PY 2016
VL 18
IS 2
BP 71
EP 77
DI 10.1111/ede.12181
PG 7
WC Evolutionary Biology; Developmental Biology; Genetics & Heredity
SC Evolutionary Biology; Developmental Biology; Genetics & Heredity
GA DI0EC
UT WOS:000373166900002
PM 26773456
ER
PT J
AU Bouchard, SS
O'Leary, CJ
Wargelin, LJ
Charbonnier, JF
Warkentin, KM
AF Bouchard, Sarah S.
O'Leary, Chelsea J.
Wargelin, Lindsay J.
Charbonnier, Julie F.
Warkentin, Karen M.
TI Post-metamorphic carry-over effects of larval digestive plasticity
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE anura; compensatory growth; complex life cycle; diet retention time; gut
plasticity; intake; juvenile; latent effects; metamorph; Neotropical
treefrog
ID CATCH-UP GROWTH; EARLY NUTRITIONAL CONDITIONS; COMPLEX LIFE-CYCLES;
COMPENSATORY GROWTH; DIFFERENTIAL PREDATION; PHENOTYPIC DEVELOPMENT;
LIPOSTATIC REGULATION; ATLANTIC SALMON; RANA-SYLVATICA; METABOLIC-RATE
AB 1. For animals with complex life cycles, conditions in the larval environment can have important effects that persist after metamorphosis. These carry-over effects may influence juvenile growth plasticity and have important fitness consequences. 2. Small juvenile red-eyed treefrogs, Agalychnis callidryas, grow faster than larger ones. We examined to what extent this growth pattern is due to carry-over effects of intraspecific larval competition. In particular, we assessed larval gut plasticity and determined whether carry-over effects could persist given the extensive gut remodelling that occurs when herbivorous larvae transition to carnivorous juveniles. 3. We reared larvae in mesocosms at low, medium and high densities and measured the size of both larval and juvenile guts, livers and fat bodies. We also monitored the timing of the onset of juvenile feeding post-metamorphosis and, after the onset of feeding, we measured intake rate and mean diet retention time. Finally, we measured juvenile metabolic rates to determine whether any organ size plasticity contributed to metabolic carry-over effects. 4. Larval density had strong effects on larval morphology with higher densities increasing gut length and decreasing liver and fat body sizes. The effects of this plasticity carried over post-metamorphosis. High larval densities produced smaller juveniles with proportionately longer guts and extremely small livers and fat bodies. There were no apparent carry-over effects on size-specific metabolic rate. 5. Differences in larval density were also associated with differences in post-metamorphic feeding. Small juveniles from high larval densities began feeding even before metamorphosis was complete, whereas large juveniles from low larval densities experienced a significant 2-week delay. Although juvenile body mass varied over threefold across treatments, once feeding was initiated, neither intake nor mean diet retention time scaled with body size. 6. Overall, high larval densities produced small juveniles with very low lipid reserves that may have stimulated hyperphagia relative to larger juveniles. Longer guts carried over from the larval stage could facilitate this by allowing small juveniles to elevate intake without sacrificing diet retention time. Patterns of intake coupled with differences in the onset of feeding explain the size-dependent growth pattern previously reported in this and other species.
C1 [Bouchard, Sarah S.; O'Leary, Chelsea J.; Wargelin, Lindsay J.] Otterbein Univ, Dept Biol & Earth Sci, 1 S Grove St, Westerville, OH 43081 USA.
[Charbonnier, Julie F.] Virginia Commonwealth Univ, Dept Biol, 1000 West Cary St, Richmond, VA 23284 USA.
[Warkentin, Karen M.] Boston Univ, Dept Biol, 5 Cummington Mall, Boston, MA 02215 USA.
[Warkentin, Karen M.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Panama.
RP Bouchard, SS (reprint author), Otterbein Univ, Dept Biol & Earth Sci, 1 S Grove St, Westerville, OH 43081 USA.
EM sbouchard@otterbein.edu
FU US National Science Foundation [DEB-0716923]; Otterbein University;
Boston University; Virginia Commonwealth University
FX We thank the Smithsonian Tropical Research Institute (STRI) for
logistical support and the use of their facilities. We also thank T.
Landberg, J. Vonesh, B. Willink and J. Touchon for valuable assistance
in the field. J. Touchon also provided statistical assistance. Funding
was provided by the US National Science Foundation (DEB-0716923 and two
Research Opportunity Award supplements), Otterbein University, Boston
University and Virginia Commonwealth University. The research was
conducted under the BU IACUC protocol 08-011 and STRI IACUC protocols
100625-1008-15 and 2011-0616-2014-04, with permits from the Autoridad
Nacional del Ambiente de Panama (SC/A-16-10 and SC/A-13-11).
NR 80
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0269-8463
EI 1365-2435
J9 FUNCT ECOL
JI Funct. Ecol.
PD MAR
PY 2016
VL 30
IS 3
BP 379
EP 388
DI 10.1111/1365-2435.12501
PG 10
WC Ecology
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GA DH7CO
UT WOS:000372949000005
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PT J
AU Calede, JJ
Samuels, JX
Chen, M
AF Calede, J. J.
Samuels, J. X.
Chen, M.
TI A multi-proxy analysis of the locomotion of entoptychine gophers
(Mammalia: Rodentia: Geomyidae) from the Oligocene of North America
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
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DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 [Calede, J. J.; Samuels, J. X.; Chen, M.] Univ Washington, Dept Biol, John Day Fossil Beds Natl Monument, Smithsonian Inst,Natl Museum Nat Hist, Seattle, WA 98195 USA.
EM caledj@uw.edu
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Collin, R
AF Chan, K. Y. K.
Collin, R.
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larval urchins to warming
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CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Hong Kong Univ Sci & Technol, Hong Kong, Hong Kong, Peoples R China.
Smithsonian Trop Res Inst, Panama City, FL USA.
EM karenchan@ust.hk
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Fredericq, S
Maslakova, S
Miglietta, MP
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Rodriguez, E
Thacker, RW
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Fredericq, S.
Maslakova, S.
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CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Smithsonian Trop Res Inst, Panama City, Panama.
Univ Louisiana Lafayette, Lafayette, LA USA.
Univ Oregon, Eugene, OR 97403 USA.
TAMU, College Stn, TX USA.
Univ Fed Parana, BR-80060000 Curitiba, Parana, Brazil.
SUNY Stony Brook, Stony Brook, NY USA.
EM CollinR@si.edu
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Harrison, L.
TI Seasonal dimorphism in gastropod hatchling size: What can we learn from
eggmass morphology and deposition site conditions?
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CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
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CY JAN 03-07, 2016
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C1 Smithsonian Trop Res Inst, Panama City, Panama.
Univ Montana, Missoula, MT 59812 USA.
EM lillian.harrison@umontana.edu
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PT J
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Strong, EE
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Strong, E. E.
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CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Univ Hawaii Hilo, Hilo, HI USA.
Smithsonian Inst, Washington, DC 20560 USA.
Natl Museum Nat Hist, London, England.
EM demainte@hawaii.edu
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MA 32-4
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PT J
AU Feo, TJ
Simon, E
Prum, RO
AF Feo, T. J.
Simon, E.
Prum, R. O.
TI When barbs get their curves: Modeling the development of barb curvature
in feathers
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SP Soc Integrat & Comparat Biol
C1 Smithsonian Inst, Washington, DC 20560 USA.
NMNH, Washington, DC USA.
Yale Univ, New Haven, CT 06520 USA.
EM FeoT@si.edu
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AU Flores, V
Page, RA
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Page, R. A.
TI The role of chemical signals in sexual selection: a novel trait in
fringe-lipped bats (Trachops cirrhosus)
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C1 Univ Chicago, Chicago, IL 60637 USA.
Smithsonian Trop Res Inst, Panama City, Panama.
EM vflores@uchicago.edu
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PT J
AU Gamboa, MP
Ghalambor, CK
Funk, WC
Sillett, TS
AF Gamboa, M. P.
Ghalambor, C. K.
Funk, W. C.
Sillett, T. S.
TI Hot Islands, Big Bills: The effect of gene flow and climate on
morphology
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SP Soc Integrat & Comparat Biol
C1 Colorado State Univ, Ft Collins, CO 80523 USA.
Smithsonian Migratory Bird Ctr, Washington, DC USA.
EM mgamboa@rams.colostate.edu
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PD MAR
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VL 56
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MA P1.103
BP E289
EP E289
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WC Zoology
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GA DH0FJ
UT WOS:000372457601514
ER
PT J
AU Kingwell, CJ
Wcislo, WT
AF Kingwell, C. J.
Wcislo, W. T.
TI The evolutionary origins of social insect queen pheromones: honesty and
dynamics of fertility signal production in a socially polyphenic
Halictid bee.
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
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DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
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CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Cornell Univ, Ithaca, NY 14853 USA.
Smithsonian Trop Res Inst, Panama City, Panama.
EM callumkingwell@gmail.com
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TC 0
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U1 2
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PU OXFORD UNIV PRESS INC
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J9 INTEGR COMP BIOL
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UT WOS:000372457601619
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PT J
AU Koetke, LJ
Devaney, J
Parker, JD
AF Koetke, L. J.
Devaney, J.
Parker, J. D.
TI Coevolved versus novel plant- herbivore interactions in a non-native
world
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CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
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CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 [Koetke, L. J.; Devaney, J.; Parker, J. D.] Smithsonian Environm Res Ctr, Edgewater, MD USA.
EM koetke@stolaf.edu
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JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 53-3
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GA DH0FJ
UT WOS:000372457600456
ER
PT J
AU Lewis, C
AF Lewis, C.
TI Differential expression of genes implicated in venom, vision and sex in
the aggregating box jellyfish Alatina alata
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
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DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
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CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Smithsonian Natl Museum Nat Hist, Washington, DC USA.
Univ Maryland, BISI BEES, Baltimore, MD USA.
EM amesc@si.edu
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UT WOS:000372457600501
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PT J
AU Lohmann, AC
Evangelista, DJ
Waldrop, LD
Mah, C
Hedrick, TL
AF Lohmann, A. C.
Evangelista, D. J.
Waldrop, L. D.
Mah, C.
Hedrick, T. L.
TI Covering ground: A look at movement patterns and random walk behavior in
Aquilonastra sea stars
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CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
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CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Univ N Carolina, Chapel Hill, NC USA.
Smithsonian Inst, Washington, DC 20560 USA.
EM alohmann@live.unc.edu
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PT J
AU Mccurry, MR
Evans, AR
Fitzgerald, MG
Shaw, M
Mchenry, CR
AF Mccurry, M. R.
Evans, A. R.
Fitzgerald, M. G.
Shaw, M.
Mchenry, C. R.
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SP Soc Integrat & Comparat Biol
C1 Natl Museum Nat Hist, London, England.
Smithsonian Inst, Washington, DC 20560 USA.
Monash Univ, Clayton, Vic 3800, Australia.
Museum Victoria, Melbourne, Vic, Australia.
Univ Newcastle, Callaghan, NSW 2308, Australia.
EM m.r.mccurry1@gmail.com
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MA 9-4
BP E144
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GA DH0FJ
UT WOS:000372457600574
ER
PT J
AU O'Mara, MT
Voigt, CC
Ter Maat, A
Pollock, HS
Burness, GP
Desantis, LM
Dechmann, DKN
AF O'Mara, M. T.
Voigt, C. C.
Ter Maat, A.
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Burness, G. P.
Desantis, L. M.
Dechmann, D. K. N.
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Tent-Making Bats
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Seewiesen, Germany.
Univ Konstanz, Dept Biol, Constance, Germany.
Smithsonian Trop Res Inst, Panama City, Panama.
Leibniz Inst Zoo & Wildlife Res, Berlin, Germany.
Max Planck Inst Ornithol, Dept Behav Neurobiol, Seewiesen, Germany.
Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL USA.
Trent Univ, Dept Biol, Peterborough, ON K9J 7B8, Canada.
EM tomara@orn.mpg.de
NR 0
TC 0
Z9 0
U1 1
U2 3
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 28-6
BP E163
EP E163
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601010
ER
PT J
AU Ren, J
Konstantinov, AS
Wang, XS
Ruan, YY
Yang, XL
Chen, R
Hu, D
Ge, S
AF Ren, Jing
Konstantinov, A. S.
Wang, X. S.
Ruan, Y. Y.
Yang, X. L.
Chen, Rui
Hu, David
Ge, Siqin
TI Camouflage Feeding: Leaf Bite Patterns Are Proportional to Beetle Body
Size
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Chinese Acad Sci, Inst Zool, Beijing, Peoples R China.
Smithsonian Inst, Washington, DC 20560 USA.
Georgia Inst Technol, Sch Mech Engn & Biol, Atlanta, GA 30332 USA.
EM renjing@ioz.ac.cn
NR 0
TC 0
Z9 0
U1 4
U2 4
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 103-5
BP E181
EP E181
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601081
ER
PT J
AU Schachat, SR
AF Schachat, S. R.
TI The evolutionary morphology of wing pattern in basal moths: implications
for the origin of butterfly symmetry systems
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 [Schachat, S. R.] Smithsonian Inst, Washington, DC 20560 USA.
EM schachatsr@si.edu
NR 0
TC 0
Z9 0
U1 1
U2 2
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA P1.106
BP E365
EP E365
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601816
ER
PT J
AU Sidlauskas, B
Alfaro, M
Burns, M
Dillman, C
Faircloth, B
Frable, B
Hoekzema, K
Melo, B
Sabaj Perez, M
Oliveira, C
Vari, R
AF Sidlauskas, B.
Alfaro, M.
Burns, M.
Dillman, C.
Faircloth, B.
Frable, B.
Hoekzema, K.
Melo, B.
Sabaj Perez, M.
Oliveira, C.
Vari, R.
TI Molecular phylogenetics, morphometrics and osteology reveal convergences
and shifts in the mode of diversification within Neotropical
headstanding fishes (Characiformes: Anostomoidea)
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Oregon State Univ, Corvallis, OR 97331 USA.
Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
Smithsonian Inst, Washington, DC 20560 USA.
Louisiana State Univ, Baton Rouge, LA 70803 USA.
Univ Estadual Paulista, Sao Paulo, Brazil.
Drexel Univ, Acad Nat Sci, Philadelphia, PA USA.
EM brian.sidlauskas@oregonstate.edu
NR 0
TC 0
Z9 0
U1 2
U2 2
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 10-3
BP E202
EP E202
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601166
ER
PT J
AU Soul, LC
Benson, RBJ
AF Soul, L. C.
Benson, R. B. J.
TI Rates and mechanisms of axial body plan evolution in Sauropterygia
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Smithsonian NMNH, Washington, DC USA.
Univ Oxford, Oxford OX1 2JD, England.
EM SoulL@si.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 21-4
BP E208
EP E208
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601189
ER
PT J
AU Steinke, KB
Collin, R
AF Steinke, K. B.
Collin, R.
TI How environmental variation affects the reproductive cycle and brood
size of a tropical Chthamalus species
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Western Washington Univ, Bellingham, WA 98225 USA.
Smithsonian Trop Res Inst, Panama City, Panama.
EM steinkk@students.wwu.edu
NR 0
TC 0
Z9 0
U1 1
U2 1
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA P2.97
BP E376
EP E376
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601860
ER
PT J
AU Wilsterman, K
Wildt, DE
Comizzoli, P
Bentley, GE
AF Wilsterman, K.
Wildt, D. E.
Comizzoli, P.
Bentley, G. E.
TI RFRP-3 expression and function in reproductive tissues of the domestic
cat (Felis catus)
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Univ Calif Berkeley, Berkeley, CA 94720 USA.
Smithsonian Conservat Biol Inst, Front Royal, VA USA.
EM kwilsterman@berkeley.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA P1.199
BP E395
EP E395
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601938
ER
PT J
AU Zattara, EE
AF Zattara, E. E.
TI Pre-existing developmental capabilities channel the evolution of novel
developmental trajectories in annelids
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Indiana Univ, Bloomington, IN 47405 USA.
Smithsonian Inst, Washington, DC 20560 USA.
EM ezattara@gmail.com
RI Zattara, Eduardo/A-3760-2012
OI Zattara, Eduardo/0000-0002-9947-9036
NR 0
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 62-1
BP E248
EP E248
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601351
ER
PT J
AU Zohdy, S
Schotte, M
AF Zohdy, S.
Schotte, M.
TI Rediscovery of Cirolana poissoni (Paulian and Delamare-Deboutteville,
1956) from Madagascar, with notes on feeding behavior
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2016
CL Portland, OR
SP Soc Integrat & Comparat Biol
C1 Auburn Univ, Auburn, AL 36849 USA.
Smithsonian Inst, Washington, DC 20560 USA.
EM sarahzohdy@gmail.com
NR 0
TC 0
Z9 0
U1 1
U2 1
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD MAR
PY 2016
VL 56
SU 1
MA 36-2
BP E250
EP E250
PG 1
WC Zoology
SC Zoology
GA DH0FJ
UT WOS:000372457601359
ER
PT J
AU Heller, EL
Kerr, KCR
Dahlan, NF
Dove, CJ
Walters, EL
AF Heller, Erin L.
Kerr, Kevin C. R.
Dahlan, Nor F.
Dove, Carla J.
Walters, Eric L.
TI Overcoming challenges to morphological and molecular identification of
Empidonax flycatchers: a case study with a Dusky Flycatcher
SO JOURNAL OF FIELD ORNITHOLOGY
LA English
DT Article
DE Barcoding; BOLD; Empidonax affinis; Empidonax oberholseri; GenBank
ID WILLOW FLYCATCHERS; TYRANNIDAE; TRAILLII
AB Flycatchers in the genus Empidonax are among the most difficult avian taxonomic groups to identify to species. Observers often rely on calls or songs in the field or detailed morphometrics in the hand to identify species. In January and February 2013, we twice captured an Empidonax flycatcher at the Virginia Zoo in Norfolk, Virginia. After being unable to identify the flycatcher to species level using morphometrics and photographs, we extracted DNA from two tail feathers collected during the second encounter to identify the individual genetically. Comparison of cytochrome c oxidase I (COI) with reference sequences in the Barcode of Life Database (BOLD) suggested that the specimen had a >99.8% probability of placement as a Dusky Flycatcher (Empidonax oberholseri). Additional comparisons of NADH dehydrogenase subunit 2 (ND2) to reference sequences in GenBank, however, suggested that the specimen was a Pine Flycatcher (Empidonax affinis), a species not represented in BOLD and confined geographically to a small area in Mexico and Guatemala. After analyzing both COI and ND2 from additional vouchered specimens, the bird caught in Virginia was determined to be a Dusky Flycatcher. We also suspect that some of the sequences in GenBank might derive from incorrectly identified specimens or otherwise could represent overlooked pseudogenes. Because the putative identification, based on GenBank sequences, would have represented the first record of Pine Flycatcher from the United States, our results reinforce the need for carefully vetted and taxonomically comprehensive molecular databases to allow definitive conclusions about sample identity. Further molecular phylogeographic review of this genus is warranted to resolve haplotype ambiguities.
RESUMEN Retos sobre la identificacion morfologica y molecular de papamoscas del genero Empidonax: un caso de estudio con Empidonax oberholseri Los papamoscas Empidonax se encuentran entre el grupo de aves mas dificiles de identificar taxonomicamente a nivel de especies. Para identificar estos pajaros, los observadores dependen, particularmente, del canto o de las llamadas o de detalles que se pueden observar cuando tienen el ave en la mano En enero y febrero del 2013, en dos ocasiones capturamos un Empidonax en el Zoologico de Virginia, Virginia. No pudimos identificar la especie utilizando fotografias o rasgos morfometricos y a tales efectos extrajimos ADN de dos de las plumas del rabo, para tratar de identificar el segundo individuo geneticamente. La comparacion de la oxidasa c citocromica I (COI), con la referencia secuencial en la base de datos del Codigo de Barras de la Vida (BOLD) sugirio que el especimen tenia >99.8% de probabilidad de ser un Empidonax oberholseri. No obstante, una comparacion de NADH dehidrogenasa, subunidad 2 (ND2) del Banco Genetico (GenBank) sugeria que el ave era Empidonax affinis, una especie que no estaba representada en BOLD y geograficamente confinada a un area pequena de Mexico y Guatemala. Luego de analizar el COI y el ND2 de especimenes adicionales, se determino que el ave capturada en Virginia era E. oberholseri. Sospechamos que la misma secuencia en el GenBank se habia obtenido de un individuo mal identificado, que de otra manera hubiera representado un pseudogene, pasado por alto. Debido a que la identificacion putativa, basado en la secuencia del GenBank, hubiera representado el primer registro de un E. affinis en los Estados Unidos, nuestros resultados apoyan la necesidad de tener mucho cuidado con las bases moleculares para permitir la identificacion conclusiva de muestras. Se necesita una revision molecular filogeografica de los Empidonax para resolver ambiguedades haplotipicas.
C1 [Heller, Erin L.; Walters, Eric L.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
[Kerr, Kevin C. R.] Toronto Zoo, 361A Old Finch Ave, Toronto, ON M1B 5K7, Canada.
[Dahlan, Nor F.; Dove, Carla J.] Smithsonian Inst, Div Birds, POB 37012,MRC 116, Washington, DC 20013 USA.
RP Walters, EL (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
EM ewalters@odu.edu
RI Walters, Eric/C-1685-2008
OI Walters, Eric/0000-0002-9414-5758
FU Virginia Academy of Science Small Project Research Funds; Virginia
Society of Ornithology JJ Murray Research Award; Old Dominion
University; U.S. Air Force; U.S. Navy; Federal Aviation Administration
FX We thank R. Sweeney and J. Lotz of the Virginia Zoo for granting us
access to mist-net and band birds, the volunteer field assistants (A.
Johnson, L. August, E. Cali, and S. Haskell) who assisted on the days
when the Dusky Flycatcher was caught, and E. Brinkley who assisted in
attempting to visually identify the bird and provided valuable input
that aided in writing this paper. We also thank S. Birks, Genetic
Resources Manager, at the Burke Museum in Seattle, WA, for sending
specimens, D. Barshis and three anonymous reviewers for comments on a
previous version of this manuscript, and G. Ritchison for helpful
suggestions to improve the manuscript. The field component of this study
was supported by awards to ELH by the Virginia Academy of Science Small
Project Research Funds and the Virginia Society of Ornithology JJ Murray
Research Award, and through start-up funds to ELW provided by Old
Dominion University. The Smithsonian Feather Lab is supported by
Interagency Agreements with the U.S. Air Force, Navy, and Federal
Aviation Administration. The research reported here was conducted under
permits from Old Dominion University, U.S. Department of the Interior,
U.S. Fish and Wildlife Service, and the Virginia Department of Game &
Inland Fisheries.
NR 25
TC 1
Z9 1
U1 5
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0273-8570
EI 1557-9263
J9 J FIELD ORNITHOL
JI J. Field Ornithol.
PD MAR
PY 2016
VL 87
IS 1
BP 96
EP 103
DI 10.1111/jofo.12132
PG 8
WC Ornithology
SC Zoology
GA DH5EB
UT WOS:000372807100009
ER
PT J
AU Sander, SJ
Siegal-Willott, JL
Ziegler, J
Lee, E
Tell, L
Murray, S
AF Sander, Samantha J.
Siegal-Willott, Jessica L.
Ziegler, Jessie
Lee, Elizabeth
Tell, Lisa
Murray, Suzan
TI PHARMACOKINETICS OF A SINGLE DOSE OF METRONIDAZOLE AFTER RECTAL
ADMINISTRATION IN CAPTIVE ASIAN ELEPHANTS (ELEPHAS MAXIMUS)
SO JOURNAL OF ZOO AND WILDLIFE MEDICINE
LA English
DT Article
DE Asian elephant; Elephas maximus; metronidazole; pharmacokinetic; rectal
ID LOXODONTA-AFRICANA; HORSES; FORMULATION; PREDICTION; CLEARANCE
AB Metronidazole is a nitroimidazole antibacterial and antiprotozoal drug with bacteriocidal activity against a broad range of anaerobic bacteria. It is a recognized treatment for elephants diagnosed with anaerobic bacterial infection or protozoal disease or exhibiting signs of colonic impaction, diarrhea, and colic. This study evaluated the pharmacokinetics of rectally administered metronidazole (15 mg/kg) in five adult female Asian elephants (Elephas maximus). Serum samples were collected from each animal for 96 hr after rectal administration of metronidazole. Serum concentrations of metronidazole and its primary metabolite, hydroxymetronidazole, were measured via ultraperformance liquid chromatography. Data were analyzed via a noncompartmental pharmacokinetic approach. Results indicated that serum levels of metronidazole were quantifiable at the 0.25 hr time point and absent in all elephants by the 96 hr time point. The serum peak concentration (mean +/- SD, 13.15 +/- 2.59 mu g/ml) and area under the curve from time 0 to infinity (mean +/- SD, 108.79 +/- 24.77 hr x mu g/ml) were higher than that reported in domestic horses after similar usage. Concurrently, the time of maximum serum concentration (mean +/- SD, 1.2 +/- 0.45 hr) and terminal elimination half-life (harmonic mean +/- pseudo-SD, 7.85 +/- 0.93 hr) were longer when compared to equine reports. Rectal administration of metronidazole was well tolerated and rapidly absorbed in all study elephants. Based on the findings in this study, metronidazole administered at a single dose of 15 mg/kg per rectum in the Asian elephant is likely to result in serum concentrations above 4 mu g/ml for 8 hr and above 2 mu g/ml for 24 hr after treatment is administered. Dosing recommendations should reflect the mean inhibitory concentration of metronidazole for each pathogen.
C1 [Sander, Samantha J.; Siegal-Willott, Jessica L.] Natl Zool Pk, Wildlife Hlth Sci, MRC 5501 Vet Hosp,POB 37012, Washington, DC 20013 USA.
[Ziegler, Jessie] Ringling Bros Ctr Elephant Conservat, 12850 Old Grade Rd, Polk City, FL 33868 USA.
[Lee, Elizabeth; Tell, Lisa] Univ Calif Davis, Sch Vet Med, Dept Med & Epidemiol, Tupper Hall,Room 2108, Davis, CA 95616 USA.
[Murray, Suzan] Natl Zool Pk, Smithsonian Conservat Biol Inst, MRC 5501 Vet Hosp,POB 37012, Washington, DC 20013 USA.
[Sander, Samantha J.] 1876 Mansion House Dr,Druid Hill Pk, Baltimore, MD 21217 USA.
RP Sander, SJ (reprint author), Natl Zool Pk, Wildlife Hlth Sci, MRC 5501 Vet Hosp,POB 37012, Washington, DC 20013 USA.; Sander, SJ (reprint author), 1876 Mansion House Dr,Druid Hill Pk, Baltimore, MD 21217 USA.
EM samantha.j.sander@gmail.com
NR 18
TC 0
Z9 0
U1 1
U2 5
PU AMER ASSOC ZOO VETERINARIANS
PI YULEE
PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA
SN 1042-7260
EI 1937-2825
J9 J ZOO WILDLIFE MED
JI J. Zoo Wildl. Med.
PD MAR
PY 2016
VL 47
IS 1
BP 1
EP 5
PG 5
WC Veterinary Sciences
SC Veterinary Sciences
GA DI0TU
UT WOS:000373211000001
PM 27010257
ER
PT J
AU Hinton, JD
Aitken-Palmer, C
Joyner, PH
Ware, L
Walsh, TF
AF Hinton, Jenna D.
Aitken-Palmer, Copper
Joyner, Priscilla H.
Ware, Lisa
Walsh, Timothy F.
TI FATAL GASTRIC DILATION IN TWO ADULT BLACK-FOOTED FERRETS (MUSTELA
NIGRIPES)
SO JOURNAL OF ZOO AND WILDLIFE MEDICINE
LA English
DT Article
DE Black-footed ferret; bloat; ferret; gastritis; Mustela nigripes; stomach
ID DILATATION-VOLVULUS; DOGS
AB Acute gastric dilation resulting in death was identified in two adult black-footed ferrets (Mustela nigripes) housed at the Smithsonian Conservation Biology Institute in Front Royal, Virginia. Both individuals were adult males (3 and 5 yr) and previously clinically healthy prior to the event. The etiology of gastric dilation in both cases could not be definitively determined, and necropsy revealed severe cardiovascular compromise secondary to bloat. Limited literature is available regarding a syndrome of this type in adult black-footed ferrets. Differential diagnoses considered included gastric dilatation volvulus (GDV), severe gastric distention of unknown origin, and gastric outflow obstruction. Given the severity of this syndrome and the findings in these two cases, acute gastric dilation should be considered in black-footed ferrets presenting with acute abdominal distention, respiratory distress, and cardiovascular compromise.
C1 [Hinton, Jenna D.] Western Univ Hlth Sci, Coll Vet Med, 309 East Second St, Pomona, CA 91766 USA.
[Aitken-Palmer, Copper; Joyner, Priscilla H.; Ware, Lisa] Smithsonian Conservat Biol Inst, Dept Conservat Med, 1500 Remount Rd, Front Royal, VA 22630 USA.
[Walsh, Timothy F.] Smithsonian Inst, Natl Zool Pk, Wildlife Hlth Serv, 3001 Connecticut Ave, Washington, DC 20008 USA.
[Hinton, Jenna D.] Pet Specialists Monterey, 451 Canyon Del Rey Blvd, Del Rey Oaks, CA 93940 USA.
RP Hinton, JD (reprint author), Western Univ Hlth Sci, Coll Vet Med, 309 East Second St, Pomona, CA 91766 USA.
EM drjennahinton@gmail.com
NR 15
TC 0
Z9 0
U1 3
U2 3
PU AMER ASSOC ZOO VETERINARIANS
PI YULEE
PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA
SN 1042-7260
EI 1937-2825
J9 J ZOO WILDLIFE MED
JI J. Zoo Wildl. Med.
PD MAR
PY 2016
VL 47
IS 1
BP 367
EP 369
PG 3
WC Veterinary Sciences
SC Veterinary Sciences
GA DI0TU
UT WOS:000373211000048
PM 27010305
ER
PT J
AU Cairns, SD
AF Cairns, Stephen D.
TI New abyssal Primnoidae (Anthozoa: Octocorallia) from the
Clarion-Clipperton Fracture Zone, equatorial northeastern Pacific
SO MARINE BIODIVERSITY
LA English
DT Article
DE Primnoidae; Clarion-clipperton fracture zone; New species; New genus;
Octocorallia; Abyssal fauna; Depth records
ID WESTERN ATLANTIC; COELENTERATA; PART; GRAY; GORGONACEA; CNIDARIA; OCEAN
AB Three new species, including a new genus, Abyssoprimnoa, are described from abyssal depths from the easternmost Clarion-Clipperton Fracture Zone in the equatorial northeastern Pacific. This prompted the listing of all 39 octocorallian taxa collected deeper than 3000 m, which constitutes only about 1.2 % of the octocoral species. To place this in perspective, the depth records for other benthic cnidarian orders are compared.
C1 [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA.
RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20560 USA.
EM cairnss@si.edu
NR 40
TC 2
Z9 2
U1 0
U2 4
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1867-1616
EI 1867-1624
J9 MAR BIODIVERS
JI Mar. Biodivers.
PD MAR
PY 2016
VL 46
IS 1
BP 141
EP 150
DI 10.1007/s12526-015-0340-x
PG 10
WC Biodiversity Conservation; Marine & Freshwater Biology
SC Biodiversity & Conservation; Marine & Freshwater Biology
GA DH9YQ
UT WOS:000373152300028
ER
PT J
AU Villarreal, AJC
Crandall-Stotler, BJ
Hart, ML
Long, DG
Forrest, LL
AF Villarreal, Juan Carlos A.
Crandall-Stotler, Barbara J.
Hart, Michelle L.
Long, David G.
Forrest, Laura L.
TI Divergence times and the evolution of morphological complexity in an
early land plant lineage (Marchantiopsida) with a slow molecular rate
SO NEW PHYTOLOGIST
LA English
DT Article
DE ancestral character reconstruction; diversification; gas exchange;
liverworts; Marchantia; slow molecular rate
ID GENE ORGANIZATION; COMPLETE SEQUENCE; FOSSIL LIVERWORT; FLOWERING
PLANTS; CHLOROPLAST DNA; LIFE-HISTORY; MODEL CHOICE; GENOME SIZE;
POLYMORPHA; ORIGIN
AB We present a complete generic-level phylogeny of the complex thalloid liverworts, a lineage that includes the model system Marchantia polymorpha. The complex thalloids are remarkable for their slow rate of molecular evolution and for being the only extant plant lineage to differentiate gas exchange tissues in the gametophyte generation. We estimated the divergence times and analyzed the evolutionary trends of morphological traits, including air chambers, rhizoids and specialized reproductive structures.
A multilocus dataset was analyzed using maximum likelihood and Bayesian approaches. Relative rates were estimated using local clocks.
Our phylogeny cements the early branching in complex thalloids. Marchantia is supported in one of the earliest divergent lineages. The rate of evolution in organellar loci is slower than for other liverwort lineages, except for two annual lineages. Most genera diverged in the Cretaceous. Marchantia polymorpha diversified in the Late Miocene, giving a minimum age estimate for the evolution of its sex chromosomes. The complex thalloid ancestor, excluding Blasiales, is reconstructed as a plant with a carpocephalum, with filament-less air chambers opening via compound pores, and without pegged rhizoids.
Our comprehensive study of the group provides a temporal framework for the analysis of the evolution of critical traits essential for plants during land colonization.
C1 [Villarreal, Juan Carlos A.; Hart, Michelle L.; Long, David G.; Forrest, Laura L.] Royal Bot Gardens Edinburgh, 20A Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland.
[Crandall-Stotler, Barbara J.] So Illinois Univ, Dept Plant Biol, Carbondale, IL 62901 USA.
[Villarreal, Juan Carlos A.] Ancon, Smithsonian Trop Res Inst, Panama City 084303092, Panama.
[Villarreal, Juan Carlos A.] Univ Laval, Dept Biol, Quebec City, PQ G1V 0A6, Canada.
RP Villarreal, AJC (reprint author), Royal Bot Gardens Edinburgh, 20A Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland.; Villarreal, AJC (reprint author), Ancon, Smithsonian Trop Res Inst, Panama City 084303092, Panama.; Villarreal, AJC (reprint author), Univ Laval, Dept Biol, Quebec City, PQ G1V 0A6, Canada.
EM jcarlos.villarreal@gmail.com
FU Scottish Government's Rural and Environment Science and Analytical
Services Division and Sibbald Trust [17]; National Science Foundation
(NSF) [EF-0531750]
FX We are grateful for funding from the Scottish Government's Rural and
Environment Science and Analytical Services Division and Sibbald Trust
Grant 2014#17 to J.C.V., and National Science Foundation (NSF) grant
EF-0531750 to B.J.C-S. Comments by three anonymous reviewers greatly
improved the manuscript.
NR 69
TC 7
Z9 7
U1 6
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0028-646X
EI 1469-8137
J9 NEW PHYTOL
JI New Phytol.
PD MAR
PY 2016
VL 209
IS 4
BP 1734
EP 1746
DI 10.1111/nph.13716
PG 13
WC Plant Sciences
SC Plant Sciences
GA DI3DY
UT WOS:000373379800038
ER
PT J
AU Nie, ZL
Funk, VA
Meng, Y
Deng, T
Sun, H
Wen, J
AF Nie, Ze-Long
Funk, Vicki A.
Meng, Ying
Deng, Tao
Sun, Hang
Wen, Jun
TI Recent assembly of the global herbaceous flora: evidence from the paper
daisies (Asteraceae: Gnaphalieae)
SO NEW PHYTOLOGIST
LA English
DT Article
DE Asteraceae; Compositae; Gnaphalieae; herbaceous flora; late
Miocene-Pliocene; open ecosystems; recent expansion
ID EXTERNAL TRANSCRIBED SPACER; FOSSIL POLLEN RECORDS;
PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; DIVERGENCE TIMES;
HELICHRYSUM ASTERACEAE; EVOLUTIONARY HISTORY; NORTHERN-HEMISPHERE;
FAMILY ASTERACEAE; MIOCENE DISPERSAL
AB The global flora is thought to contain a large proportion of herbs, and understanding the general spatiotemporal processes that shaped the global distribution of these communities is one of the most difficult issues in biogeography.
We explored patterns of world-wide biogeography in a species-rich herbaceous group, the paper daisy tribe Gnaphalieae (Asteraceae), based on the hitherto largest taxon sampling, a total of 835 terminal accessions representing 80% of the genera, and encompassing the global geographic range of the tribe, with nuclear internal transcribed spacer (ITS) and external transcribed spacer (ETS) sequences.
Biogeographic analyses indicate that Gnaphalieae originated in southern Africa during the Oligocene, followed by repeated migrations into the rest of Africa and the Mediterranean region, with subsequent entries into other continents during various periods starting in the Miocene.
Expansions in the late Miocene to Pliocene appear to have been the driving force that shaped the global distribution of the tribe as forests were progressively broken up by the mid-continent aridification and savannas and grasslands expanded into the interior of the major continents. This pattern of recent colonizations may explain the world-wide distribution of many other organisms in open ecosystems and it is highlighted here as an emerging pattern in the evolution of the global flora.
C1 [Nie, Ze-Long; Meng, Ying] Jishou Univ, Coll Biol & Environm Sci, Key Lab Plant Resources Conservat & Utilizat, Jishou 416000, Hunan, Peoples R China.
[Nie, Ze-Long; Meng, Ying; Deng, Tao; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Plant Div & Biogeog East Asia, Kunming 650201, Yunnan, Peoples R China.
[Funk, Vicki A.; Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA.
RP Sun, H (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Plant Div & Biogeog East Asia, Kunming 650201, Yunnan, Peoples R China.; Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA.
EM sunhang@mail.kib.ac.cn; wenj@si.edu
FU Strategic Priority Research Program of the Chinese Academy of Sciences
[XDB03030112]; Natural Sciences Foundation of China (NSFC) [31570211,
31129001]; United Fund of the NSFC and Yunnan Natural Science Foundation
[U1136601]; CAS/SAFEA International Partnership Program for Creative
Research Teams; John D. and Catherine T. MacArthur Foundation;
Laboratories of Analytical Biology of the National Museum of Natural
History, Smithsonian Institution; Small Grants Program of the National
Museum of Natural History, Smithsonian Institution; Smithsonian
Postdoctoral Fellowship
FX This study was supported by grants from the Strategic Priority Research
Program (B) of the Chinese Academy of Sciences (XDB03030112 to H.S.),
the Natural Sciences Foundation of China (NSFC, 31570211 to Z-L.N. and
31129001 to J.W.), the United Fund of the NSFC and Yunnan Natural
Science Foundation (U1136601 to H.S.), the CAS/SAFEA International
Partnership Program for Creative Research Teams (to H.S.), and the John
D. and Catherine T. MacArthur Foundation (to J.W.). Laboratory work was
carried out at and partially supported by the Laboratories of Analytical
Biology of the National Museum of Natural History, Smithsonian
Institution. Fieldwork and lab work in North America were supported by
the Small Grants Program of the National Museum of Natural History,
Smithsonian Institution. Z-L.N. was awarded a Smithsonian Postdoctoral
Fellowship in 2011-2012.
NR 117
TC 5
Z9 6
U1 6
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0028-646X
EI 1469-8137
J9 NEW PHYTOL
JI New Phytol.
PD MAR
PY 2016
VL 209
IS 4
BP 1795
EP 1806
DI 10.1111/nph.13740
PG 12
WC Plant Sciences
SC Plant Sciences
GA DI3DY
UT WOS:000373379800043
PM 26528674
ER
PT J
AU Chakraborti, S
Childs, F
Soderberg, A
AF Chakraborti, Sayan
Childs, Francesca
Soderberg, Alicia
TI YOUNG REMNANTS OF TYPE Ia SUPERNOVAE AND THEIR PROGENITORS: A STUDY OF
SNR G1.9+0.3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; circumstellar matter; ISM: individual objects (SNR
G1.9+0.3); ISM: supernova remnants; radio continuum: general;
supernovae: general; X-rays: general
ID X-RAY-EMISSION; WHITE-DWARF MODELS; CIRCUMSTELLAR INTERACTION;
LIGHT-CURVE; RADIO; EVOLUTION; MASS; EXPANSION; BINARIES; UNIVERSE
AB SNe Ia, with their remarkably homogeneous light curves and spectra, have been used as standardizable candles to measure the accelerating expansion of the universe. Yet, their progenitors remain elusive. Common explanations invoke a degenerate star (white dwarf) that explodes upon almost reaching the Chandrasekhar limit, by either steadily accreting mass from a companion star or violently merging with another degenerate star. We show that circumstellar interaction in young Galactic supernova remnants can be used to distinguish between these single and double degenerate (DD) progenitor scenarios. Here we propose a new diagnostic, the surface brightness index, which can be computed from theory and compared with Chandra and Very Large Array (VLA) observations. We use this method to demonstrate that a DD progenitor can explain the decades-long flux rise and size increase of the youngest known galactic supernova remnant (SNR), G1.9+0.3. We disfavor a single degenerate scenario for SNR G1.9+0.3. We attribute the observed properties to the interaction between a steep ejecta profile and a constant density environment. We suggest using the upgraded VLA, ASKAP, and MeerKAT to detect circumstellar interaction in the remnants of historical SNe Ia in the Local Group of galaxies. This may settle the long-standing debate over their progenitors.
C1 [Chakraborti, Sayan; Childs, Francesca; Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Chakraborti, Sayan] Harvard Univ, Soc Fellows, Cambridge, MA 02138 USA.
[Childs, Francesca] Harvard Univ, Harvard Coll, Cambridge, MA 02138 USA.
[Soderberg, Alicia] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
RP Chakraborti, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.; Chakraborti, S (reprint author), Harvard Univ, Soc Fellows, Cambridge, MA 02138 USA.
EM schakraborti@post.harvard.edu
NR 50
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 37
DI 10.3847/0004-637X/819/1/37
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400037
ER
PT J
AU Civano, F
Marchesi, S
Comastri, A
Urry, MC
Elvis, M
Cappelluti, N
Puccetti, S
Brusa, M
Zamorani, G
Hasinger, G
Aldcroft, T
Alexander, DM
Allevato, V
Brunner, H
Capak, P
Finoguenov, A
Fiore, F
Fruscione, A
Gilli, R
Glotfelty, K
Griffiths, RE
Hao, H
Harrison, FA
Jahnke, K
Kartaltepe, J
Karim, A
LaMassa, SM
Lanzuisi, G
Miyaji, T
Ranalli, P
Salvato, M
Sargent, M
Scoville, NJ
Schawinski, K
Schinnerer, E
Silverman, J
Smolcic, V
Stern, D
Toft, S
Trakhenbrot, B
Treister, E
Vignali, C
AF Civano, F.
Marchesi, S.
Comastri, A.
Urry, M. C.
Elvis, M.
Cappelluti, N.
Puccetti, S.
Brusa, M.
Zamorani, G.
Hasinger, G.
Aldcroft, T.
Alexander, D. M.
Allevato, V.
Brunner, H.
Capak, P.
Finoguenov, A.
Fiore, F.
Fruscione, A.
Gilli, R.
Glotfelty, K.
Griffiths, R. E.
Hao, H.
Harrison, F. A.
Jahnke, K.
Kartaltepe, J.
Karim, A.
LaMassa, S. M.
Lanzuisi, G.
Miyaji, T.
Ranalli, P.
Salvato, M.
Sargent, M.
Scoville, N. J.
Schawinski, K.
Schinnerer, E.
Silverman, J.
Smolcic, V.
Stern, D.
Toft, S.
Trakhenbrot, B.
Treister, E.
Vignali, C.
TI THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; cosmology: observations; galaxies: evolution; quasars:
general; surveys; X-rays: general
ID WIDE-FIELD SURVEY; ACTIVE GALACTIC NUCLEI; EVOLUTION SURVEY COSMOS; MS
SOURCE CATALOGS; X-RAY SURVEY; XMM-NEWTON; BLACK-HOLE; NUMBER COUNTS;
STRIPE 82; LOG S
AB The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg(2) of the COSMOS field with an effective exposure of similar or equal to 160 ks over the central 1.5 deg(2) and of similar or equal to 80 ks in the remaining area. The survey is the combination of 56 new observations obtained as an X-ray Visionary Project with the previous C-COSMOS survey. We describe the reduction and analysis of the new observations and the properties of 2273 point sources detected above a spurious probability of 2 x 10(-5). We also present the updated properties of the C-COSMOS sources detected in the new data. The whole survey includes 4016 point sources (3814, 2920 and 2440 in the full, soft, and hard band). The limiting depths are 2.2 x 10(-16), 1.5 x 10(-15), and 8.9 x 10(-16) erg cm(-2) s(-1)in the 0.5-2, 2-10, and 0.5-10 keV bands, respectively. The observed fraction of obscured active galactic nuclei with a column density >10(22) cm(-2) from the hardness ratio (HR) is similar to 50(-16)(+17)%. Given the large sample we compute source number counts in the hard and soft bands, significantly reducing the uncertainties of 5%-10%. For the first time we compute number counts for obscured (HR > -0.2) and unobscured (HR < -0.2) sources and find significant differences between the two populations in the soft band. Due to the unprecedent large exposure, COSMOS-Legacy area is three times larger than surveys at similar depths and its depth is three times fainter than surveys covering similar areas. The area-flux region occupied by COSMOS-Legacy is likely to remain unsurpassed for years to come.
C1 [Civano, F.; Marchesi, S.; Urry, M. C.; LaMassa, S. M.] Yale Univ, Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA.
[Civano, F.; Marchesi, S.; Elvis, M.; Aldcroft, T.; Fruscione, A.; Glotfelty, K.; Hao, H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Marchesi, S.; Brusa, M.; Lanzuisi, G.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Comastri, A.; Cappelluti, N.; Brusa, M.; Zamorani, G.; Gilli, R.; Lanzuisi, G.; Vignali, C.] INAF Osservatorio Astronom Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Puccetti, S.] ASDC ASI, Via Politecn, I-00133 Rome, Italy.
[Hasinger, G.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Allevato, V.; Finoguenov, A.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, FI-00014 Helsinki, Finland.
[Brunner, H.; Salvato, M.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Capak, P.] IPAC, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Capak, P.; Scoville, N. J.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Fiore, F.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Griffiths, R. E.] Univ Hawaii, Div Nat Sci, Dept Phys & Astron, 200 W Kawili St, Hilo, HI 96720 USA.
[Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Jahnke, K.; Schinnerer, E.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Kartaltepe, J.] Natl Opt Astron Observ, 950N Cherry Ave, Tucson, AZ 85719 USA.
[Kartaltepe, J.] Rochester Inst Technol, Sch Phys & Astron, 84 Lomb Mem Dr, Rochester, NY 14623 USA.
[Karim, A.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
[Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Km 103,Carret Tijunana Ensenada, Ensenada, Baja California, Mexico.
[Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Ranalli, P.] Natl Observ Athens, AASARS, Penteli 15236, Greece.
[Sargent, M.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Schawinski, K.; Trakhenbrot, B.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Schinnerer, E.] Natl Radio Astron Observ, Pete V Domenici Sci Operat Ctr, 1003 Lopezville Rd, Socorro, NM 87801 USA.
[Silverman, J.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Smolcic, V.] Univ Zagreb, Dept Phys, Bijeniaa Cesta 32, HR-10000 Zagreb, Croatia.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Toft, S.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Mariesvej 30, DK-2100 Copenhagen, Denmark.
[Treister, E.] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile.
RP Civano, F (reprint author), Yale Univ, Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA.
RI Ranalli, Piero/K-6363-2013;
OI Ranalli, Piero/0000-0003-3956-755X; Lanzuisi,
Giorgio/0000-0001-9094-0984; Cappelluti, Nico/0000-0002-1697-186X;
Zamorani, Giovanni/0000-0002-2318-301X; Urry, Meg/0000-0002-0745-9792;
Trakhtenbrot, Benny/0000-0002-3683-7297; Schinnerer,
Eva/0000-0002-3933-7677
FU NASA [G07-8136A, NAS8-03060, NNX15AE61G]; PRIN-INAF; FP7 Career
Integration Grant "eEASy" [CIG 321913]; UNAM-DGAPA [PAPIIT IN104113];
CONACyT [179662]; Collaborative Research Council [956]; Deutsche
Forschungsgemeinschaft; Greek General Secretariat of Research and
Technology; Science and Technology Facilities Council [ST/I001573/1];
Swiss National Science Foundation [PP00P2_138979/1]; Center of
Excellence in Astrophysics and Associated Technologies [PFB 06];
FONDECYT [1120061]; CONICYT [ACT1101]; European Union [337595, 333654];
Danish National Research Foundation
FX This work was supported in part by NASA Chandra grant number G07-8136A
(F.C., S.M., V.A., M.E., H.S.); PRIN-INAF 2014 "Windy Black Holes
combing galaxy evolution" (A.C., M.B., G.L. and C.V.); the FP7 Career
Integration Grant "eEASy": "Supermassive blackholes through cosmic time:
from current surveys to eROSITA-Euclid Synergies"(CIG 321913; M.B. and
G.L.); UNAM-DGAPA Grant PAPIIT IN104113 and CONACyT Grant Cientifica
Basica #179662 (T.M.); Collaborative Research Council 956, sub-project
A1, funded by the Deutsche Forschungsgemeinschaft (A.K.); NASA contract
NAS8-03060 (T.A., A.F., K.G.); the Greek General Secretariat of Research
and Technology in the framework of the Programme of Support of
Postdoctoral Researchers (P.R.); NASA award NNX15AE61G (R.G.); the
Science and Technology Facilities Council through grant code
ST/I001573/1 (D.M.A.); the Swiss National Science Foundation Grant
PP00P2_138979/1 (K.S.); the Center of Excellence in Astrophysics and
Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061
and by the CONICYT Anillo project ACT1101 (E.T.); the European Union's
Seventh Framework Programme under grant agreements 337595 (ERC Starting
Grant, "CoSMass") and 333654 (CIG, AGN feedback; V.S.). S.T. is part of
The Dark Cosmology Centre, funded by the Danish National Research
Foundation. B.T. is a Zwicky Fellow.
NR 64
TC 18
Z9 18
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 62
DI 10.3847/0004-637X/819/1/62
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400062
ER
PT J
AU Cleeves, LI
Bergin, EA
Alexander, CMO
Du, FJ
Graninger, D
Oberg, KI
Harries, TJ
AF Cleeves, L. Ilsedore
Bergin, Edwin A.
Alexander, Conel M. O'D.
Du, Fujun
Graninger, Dawn
Oeberg, Karin I.
Harries, Tim J.
TI EXPLORING THE ORIGINS OF DEUTERIUM ENRICHMENTS IN SOLAR NEBULAR ORGANICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; astrochemistry; circumstellar matter; stars:
pre-main sequence
ID LOW-MASS PROTOSTARS; POLYCYCLIC AROMATIC-HYDROCARBONS; PROTOPLANETARY
DISKS. II.; COMET 103P/HARTLEY 2; D/H RATIO; PRIMITIVE METEORITES;
DEUTERATED WATER; LOW-TEMPERATURES; RAY IONIZATION; COSMIC-RAYS
AB Deuterium-to-hydrogen (D/H) enrichments in molecular species provide clues about their original formation environment. The organic materials in primitive solar system bodies generally have higher D/H ratios and show greater D/H variation when compared to D/H in solar system water. We propose this difference arises at least in part due to (1) the availability of additional chemical fractionation pathways for organics beyond that for water, and (2) the higher volatility of key carbon reservoirs compared to oxygen. We test this hypothesis using detailed disk models, including a sophisticated, new disk ionization treatment with a low cosmic-ray ionization rate, and find that disk chemistry leads to higher deuterium enrichment in organics compared to water, helped especially by fractionation via the precursors CH2D+/CH3+. We also find that the D/H ratio in individual species varies significantly depending on their particular formation pathways. For example, from similar to 20-40 au, CH4 can reach D/H similar to 2 x 10(-3), while D/H in CH3OH remains locally unaltered. Finally, while the global organic D/H in our models can reproduce intermediately elevated D/H in the bulk hydrocarbon reservoir, our models are unable to reproduce the most deuterium-enriched organic materials in the solar system, and thus our model requires some inheritance from the cold interstellar medium from which the Sun formed.
C1 [Cleeves, L. Ilsedore; Graninger, Dawn; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bergin, Edwin A.; Du, Fujun] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Alexander, Conel M. O'D.] Carnegie Inst Sci, DTM, Washington, DC 20015 USA.
[Harries, Tim J.] Univ Exeter, Dept Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England.
RP Cleeves, LI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ilse.cleeves@cfa.harvard.edu
OI Alexander, Conel/0000-0002-8558-1427; Cleeves, L.
Ilsedore/0000-0003-2076-8001
FU NSF [AST-1008800]; Rackham Predoctoral Fellowship; NASA [NNX14AJ54G, NAS
5-26555]; NASA Origins of Solar Systems Program [NNX12A193G]; STFC
[ST/M00127X/1]; Simons Collaboration on the Origins of Life (SCOL); NASA
through Hubble Fellowship grant by Space Telescope Science Institute
[HST-HF2-51356.001-A]
FX The authors are thoroughly grateful to the anonymous referee, whose
comments and careful consideration significantly improved the
manuscript. L.I.C. and E.A.B. acknowledge the support of NSF grant
AST-1008800 and the Rackham Predoctoral Fellowship. C.A. was partially
supported by NASA Cosmochemistry grant NNX14AJ54G. F.D. and E.A.B.
acknowledge support of grant NNX12A193G from the NASA Origins of Solar
Systems Program. T.J.H. acknowledges support from STFC Consolidated
Grant ST/M00127X/1. K.I.O. also acknowledges funding from the Simons
Collaboration on the Origins of Life (SCOL). Support for the writing of
this manuscript was provided by NASA through Hubble Fellowship grant
HST-HF2-51356.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555.
NR 67
TC 3
Z9 3
U1 2
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 13
DI 10.3847/0004-637X/819/1/13
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400013
ER
PT J
AU Garcia, JA
Grinberg, V
Steiner, JF
McClintock, JE
Pottschmidt, K
Rothschild, RE
AF Garcia, Javier A.
Grinberg, Victoria
Steiner, James F.
McClintock, Jeffrey E.
Pottschmidt, Katja
Rothschild, Richard E.
TI AN EMPIRICAL METHOD FOR IMPROVING THE QUALITY OF RXTE HEXTE SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; space vehicles: instruments; X-rays:
individual (Crab, XTE J1752-223, GX 339-4)
ID RAY-TIMING-EXPLORER; HARD X-RAY; CRAB-NEBULA
AB We have developed a correction tool to improve the quality of Rossi X-ray Timing Explorer (RXTE) High Energy X-ray Timing Experiment (HEXTE) spectra by employing the same method we used earlier to improve the quality of RXTE Proportional Counter Array (PCA) spectra. We fit all of the hundreds of HEXTE spectra of the Crab individually to a simple power-law model, some 37. million counts in total for Cluster. A and 39. million counts for Cluster. B, and we create for each cluster a combined spectrum of residuals. We find that the residual spectrum of Cluster. A is free of instrumental artifacts while that of Cluster B contains significant features with amplitudes similar to 1%; the most prominent is in the energy range 30-50 keV, which coincides with the iodine K edge. Starting with the residual spectrum for Cluster. B, via an iterative procedure we created the calibration tool HEXBCORR for correcting any Cluster. B spectrum of interest. We demonstrate the efficacy of the tool by applying it to Cluster. B spectra of two bright black holes, which contain several million counts apiece. For these spectra, application of the tool significantly improves the goodness of fit, while affecting only slightly the broadband fit parameters. The tool may be important for the study of spectral features, such as cyclotron lines, a topic that is beyond the scope of this paper.
C1 [Garcia, Javier A.; Steiner, James F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Grinberg, Victoria; Steiner, James F.] MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.
[Pottschmidt, Katja] UMBC, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Garcia, JA; Steiner, JF; McClintock, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Grinberg, V; Steiner, JF (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.; Pottschmidt, K (reprint author), UMBC, Dept Phys, Baltimore, MD 21250 USA.; Pottschmidt, K (reprint author), UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.; Pottschmidt, K (reprint author), CRESST, Greenbelt, MD 20771 USA.; Pottschmidt, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Rothschild, RE (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
EM javier@head.cfa.harvard.edu; grinberg@space.mit.edu; jsteiner@mit.edu;
jem@cfa.harvard.edu; katja@milkyway.gsfc.nasa.gov; rrothschild@ucsd.edu
FU CGPS grant from Smithsonian Institution; NASA Hubble Fellowship
[HST-HF-51315.01]; NASA Einstein Fellowship [PF5-160144]; NASA through
Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; NASA
[NAS8-03060]
FX We thank an anonymous referee for several helpful comments. J.G. and
J.E.M. acknowledge the support of a CGPS grant from the Smithsonian
Institution. J.F.S. has been supported by NASA Hubble Fellowship grant
HST-HF-51315.01 and NASA Einstein Fellowship grant PF5-160144. V.G.
acknowledges support provided by NASA through the Smithsonian
Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of
the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated
by SAO for and on behalf of NASA under contract NAS8-03060.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 76
DI 10.3847/0004-637X/819/1/76
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400076
ER
PT J
AU MacLeod, M
Guillochon, J
Ramirez-Ruiz, E
Kasen, D
Rosswog, S
AF MacLeod, Morgan
Guillochon, James
Ramirez-Ruiz, Enrico
Kasen, Daniel
Rosswog, Stephan
TI OPTICAL THERMONUCLEAR TRANSIENTS FROM TIDAL COMPRESSION OF WHITE DWARFS
AS TRACERS OF THE LOW END OF THE MASSIVE BLACK HOLE MASS FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; methods: numerical;
radiative transfer; white dwarfs
ID GAMMA-RAY BURST; EARLY-TYPE GALAXIES; IA SUPERNOVAE; X-RAY; SWIFT
J1644+57; GRAVITATIONAL-WAVES; DISRUPTION FLARES; GLOBULAR-CLUSTERS;
STAR DISTRIBUTION; LIGHT CURVES
AB In this paper, we model the observable signatures of tidal disruptions of white dwarf (WD) stars using massive black holes (MBHs) of moderate mass, approximate to 10(3)-10(5) M-circle dot. When the WD passes deep enough within the MBH's tidal field, these signatures include thermonuclear transients from burning during maximum compression. We combine a hydrodynamic simulation that includes nuclear burning of the disruption of a 0.6 M-circle dot C/O WD with a Monte Carlo radiative transfer calculation to synthesize the properties of a representative transient. The transient's emission emerges in the optical, with light. curves and spectra reminiscent of Type I supernovae. The properties are strongly viewing. angle dependent, and key spectral signatures are approximate to 10,000 km s(-1) doppler shifts, due to the orbital motion of the unbound ejecta. Disruptions of He WDs likely produce large quantities of intermediate-mass elements, offering a possible production mechanism for Ca-rich transients. Accompanying multi-wavelength transients are fueled by accretion and arise from the nascent accretion disk and relativistic jet. If MBHs of moderate mass exist with number densities similar to those of supermassive BHs, both high-energy wide-field monitors and upcoming optical surveys should detect tens to hundreds of WD tidal disruptions per year. The current best strategy for their detection may therefore be deep optical follow-up of high-energy transients of unusually long duration. The detection rate or the nondetection of these transients by current and upcoming surveys can thus be used to place meaningful constraints on the extrapolation of the MBH mass function to moderate masses.
C1 [MacLeod, Morgan; Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Guillochon, James] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Nucl Sci, Berkeley, CA 94720 USA.
[Rosswog, Stephan] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
RP MacLeod, M (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
OI Guillochon, James/0000-0002-9809-8215
FU UCSC; Packard Foundation; Radcliffe Institute for Advanced Study; NASA
ATP grant [NNX14AH37G]; Einstein Grant [PF3-140108]; DFG [RO-3399/8-1,
AOBJ-575415]; Swedish Research Council (VR) [621-2012-4870]
FX We thank Maria Drout for guidance and data used in Figure 6, and Ryan
Foley for helpful discussions and comments on an early version of this
manuscript. We are grateful to Laura Chomiuk and Sjoert van Velzen for
comments on radio afterglows of tidal disruption events and to Sjoert
van Velzen for sharing code to estimate their properties. We further
acknowledge helpful conversations with Roseanne Cheng, Lixin Dai, Julian
Krolik, Tom Maccarone, Phillip Macias, Michela Mapelli, Cole Miller,
Dheeraj Pasham, Martin Rees, Elena Rossi, and Michele Trenti. M.M. is
grateful for the support of the Chancellor's Fellowship at UCSC. E.R.-R.
acknowledges financial support from the Packard Foundation, Radcliffe
Institute for Advanced Study, and NASA ATP grant NNX14AH37G. J.G.
acknowledges support from Einstein Grant PF3-140108. S.R. was supported
by the DFG under RO-3399/8-1, AOBJ-575415 and by the Swedish Research
Council (VR) under grant 621-2012-4870. Part of the simulations have
been performed at the facilities of the The North-German Supercomputing
Alliance (HLRN).
NR 119
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 3
DI 10.3847/0004-637X/819/1/3
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400003
ER
PT J
AU Pober, JC
Hazelton, BJ
Beardsley, AP
Barry, NA
Martinot, ZE
Sullivan, IS
Morales, MF
Bell, ME
Bernardi, G
Bhat, NDR
Bowman, JD
Briggs, F
Cappall, RJ
Carroll, P
Corey, BE
de Oliveira-Costar, A
Deshpande, AA
Dillon, JS
Emrich, D
Ewall-Wice, AM
Feng, L
Goeke, R
Greenhill, LJ
Hewitt, JN
Hindson, L
Hurley-Walker, N
Jacobs, DC
Johnston-Hollitt, M
Kaplan, DL
Kasper, JC
Kim, HS
Kittiwisit, P
Kratzenberg, E
Kudryavtseva, N
Lenc, E
Line, J
Loeb, A
Lonsdale, CJ
Lynch, MJ
McKinley, B
McWhirter, SR
Mitchell, DA
Morgan, E
Neben, AR
Oberoi, D
Offringa, AR
Ord, SM
Paul, S
Pindor, B
Prabu, T
Procopio, P
Riding, J
Rogers, AEE
Roshi, A
Sethi, SK
Shankar, NU
Srivani, KS
Subrahmanyan, R
Tegmark, M
Thyagarajan, N
Tingay, SJ
Trott, CM
Waterson, M
Wayth, RB
Webster, RL
Whitney, AR
Williams, A
Williams, CL
Wyithe, JSB
AF Pober, J. C.
Hazelton, B. J.
Beardsley, A. P.
Barry, N. A.
Martinot, Z. E.
Sullivan, I. S.
Morales, M. F.
Bell, M. E.
Bernardi, G.
Bhat, N. D. R.
Bowman, J. D.
Briggs, F.
Cappall, R. J.
Carroll, P.
Corey, B. E.
de Oliveira-Costar, A.
Deshpande, A. A.
Dillon, Joshua S.
Emrich, D.
Ewall-Wice, A. M.
Feng, L.
Goeke, R.
Greenhill, L. J.
Hewitt, J. N.
Hindson, L.
Hurley-Walker, N.
Jacobs, D. C.
Johnston-Hollitt, M.
Kaplan, D. L.
Kasper, J. C.
Kim, Han-Seek
Kittiwisit, P.
Kratzenberg, E.
Kudryavtseva, N.
Lenc, E.
Line, J.
Loeb, A.
Lonsdale, C. J.
Lynch, M. J.
McKinley, B.
McWhirter, S. R.
Mitchell, D. A.
Morgan, E.
Neben, A. R.
Oberoi, D.
Offringa, A. R.
Ord, S. M.
Paul, Sourabh
Pindor, B.
Prabu, T.
Procopio, P.
Riding, J.
Rogers, A. E. E.
Roshi, A.
Sethi, Shiv K.
Shankar, N. Udaya
Srivani, K. S.
Subrahmanyan, R.
Tegmark, M.
Thyagarajan, Nithyanandan
Tingay, S. J.
Trott, C. M.
Waterson, M.
Wayth, R. B.
Webster, R. L.
Whitney, A. R.
Williams, A.
Williams, C. L.
Wyithe, J. S. B.
TI THE IMPORTANCE OF WIDE-FIELD FOREGROUND REMOVAL FOR 21 cm COSMOLOGY: A
DEMONSTRATION WITH EARLY MWA EPOCH OF REIONIZATION OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark ages, reionization, first stars;
techniques: interferometric
ID MURCHISON WIDEFIELD ARRAY; LARGE-SCALE STRUCTURES; POWER SPECTRUM;
LOW-FREQUENCY; RADIO INTERFEROMETRY; TO 0.8; SUBTRACTION; CALIBRATION;
EMISSION; FLUCTUATIONS
AB In this paper we present observations, simulations, and analysis demonstrating the direct connection between the location of foreground emission on the sky and its location in cosmological power spectra from interferometric redshifted 21 cm experiments. We begin with a heuristic formalism for understanding the mapping of sky coordinates into the cylindrically averaged power spectra measurements used by 21 cm experiments, with a focus on the effects of the instrument beam response and the associated sidelobes. We then demonstrate this mapping by analyzing power spectra with both simulated and observed data from the Murchison Widefield Array. We find that removing a foreground model that includes sources in both the main field of view and the first sidelobes reduces the contamination in high k(parallel to) modes by several per cent relative to a model that only includes sources in the main field of view, with the completeness of the foreground model setting the principal limitation on the amount of power removed. While small, a percent-level amount of foreground power is in itself more than enough to prevent recovery of any Epoch of Reionization signal from these modes. This result demonstrates that foreground subtraction for redshifted 21 cm experiments is truly a wide-field problem, and algorithms and simulations must extend beyond the instrument's main field of view to potentially recover the full 21 cm power spectrum.
C1 [Pober, J. C.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Pober, J. C.; Hazelton, B. J.; Beardsley, A. P.; Barry, N. A.; Martinot, Z. E.; Sullivan, I. S.; Morales, M. F.; Carroll, P.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Beardsley, A. P.; Bowman, J. D.; Jacobs, D. C.; Kittiwisit, P.; Thyagarajan, Nithyanandan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Bell, M. E.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa.
[Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Bernardi, G.; Greenhill, L. J.; Kasper, J. C.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bhat, N. D. R.; Emrich, D.; Hurley-Walker, N.; Kudryavtseva, N.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Bhat, N. D. R.; Kim, Han-Seek; Lenc, E.; Line, J.; Mitchell, D. A.; Offringa, A. R.; Ord, S. M.; Pindor, B.; Subrahmanyan, R.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Webster, R. L.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT, Australia.
[Briggs, F.; McKinley, B.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Cappall, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA.
[de Oliveira-Costar, A.; Feng, L.; Goeke, R.; Hewitt, J. N.; Morgan, E.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Deshpande, A. A.; Paul, Sourabh; Prabu, T.; Sethi, Shiv K.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Dillon, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dillon, Joshua S.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Dillon, Joshua S.; Ewall-Wice, A. M.; Feng, L.; Hewitt, J. N.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Hindson, L.; Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Kaplan, D. L.] Univ Wisconsin Milwaukee, Dept Phys, Milwaukee, WI 53201 USA.
[Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Kim, Han-Seek; Line, J.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Mitchell, D. A.] CSIRO Astron & Space Sci CASS, POB 76, Epping, NSW 1710, Australia.
[Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA.
[Roshi, A.] Natl Radio Astron Observ, Green Bank, WV USA.
[Waterson, M.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England.
[Pober, J. C.] Natl Sci Fdn, Astron & Astrophys, 4201 Wilson Blvd, Arlington, VA 22230 USA.
RP Pober, JC (reprint author), Brown Univ, Dept Phys, Providence, RI 02912 USA.
RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Deshpande,
Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Sethi,
Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012;
OI Wayth, Randall/0000-0002-6995-4131; PINDOR, BARTOSZ/0000-0003-3240-2437;
Wyithe, Stuart/0000-0001-7956-9758; /0000-0002-0086-7363; Pober,
Jonathan/0000-0002-3492-0433; Trott, Cathryn/0000-0001-6324-1766; Lenc,
Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942
FU NSF Astronomy and Astrophysics Fellowship [AST-1302774]; U.S. National
Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753,
AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938];
U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre
for All-sky Astrophysics (an Australian Research Council Centre of
Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT
School of Science; Raman Research Institute; Australian National
University; Victoria University of Wellington (New Zealand Ministry of
Economic Development) [MED-E1799]; Victoria University of Wellington
(IBM Shared University Research Grant); Australian Federal government
via Commonwealth Scientific and Industrial Research Organization
(CSIRO); National Collaborative Research Infrastructure Strategy;
Education Investment Fund; Australia India Strategic Research Fund;
Astronomy Australia Limited; NVIDIA at Harvard University; International
Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin
University; University of Western Australia; Western Australian State
government
FX The authors wish to thank Adrian Liu for helpful conversations and our
referee for a number of helpful suggestions that improved the paper.
J.C.P. is supported by an NSF Astronomy and Astrophysics Fellowship
under award AST-1302774. This scientific work makes use of the Murchison
Radio-astronomy Observatory, operated by CSIRO. We acknowledge the
Wajarri Yamatji people as the traditional owners of the Observatory
site. Support for the MWA comes from the U.S. National Science
Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and
AST-0908884), the Australian Research Council (LIEF grants LE0775621 and
LE0882938), the U.S. Air Force Office of Scientific Research (grant
FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian
Research Council Centre of Excellence funded by grant CE110001020).
Support is also provided by the Smithsonian Astrophysical Observatory,
the MIT School of Science, the Raman Research Institute, the Australian
National University, and the Victoria University of Wellington (via
grant MED-E1799 from the New Zealand Ministry of Economic Development
and an IBM Shared University Research Grant). The Australian Federal
government provides additional support via the Commonwealth Scientific
and Industrial Research Organization (CSIRO), National Collaborative
Research Infrastructure Strategy, Education Investment Fund, and the
Australia India Strategic Research Fund, and Astronomy Australia
Limited, under contract to Curtin University. We acknowledge the iVEC
Petabyte Data Store, the Initiative in Innovative Computing and the CUDA
Center for Excellence sponsored by NVIDIA at Harvard University, and the
International Centre for Radio Astronomy Research (ICRAR), a Joint
Venture of Curtin University and The University of Western Australia,
funded by the Western Australian State government.
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JI Astrophys. J.
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DI 10.3847/0004-637X/819/1/8
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400008
ER
PT J
AU Rines, KJ
Geller, MJ
Diaferio, A
Hwang, HS
AF Rines, Kenneth J.
Geller, Margaret J.
Diaferio, Antonaldo
Hwang, Ho Seong
TI HeCS-SZ: THE HECTOSPEC SURVEY OF SUNYAEV-ZELDOVICH-SELECTED CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; galaxies:
distances and redshifts; galaxies: kinematics and dynamics
ID DIGITAL SKY SURVEY; X-RAY MEASUREMENTS; MASSIVE GALAXY CLUSTERS;
SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; SCALING RELATIONS; VELOCITY
DISPERSIONS; COSMOLOGICAL CONSTRAINTS; PRESSURE PROFILES; OBSERVED
GROWTH
AB We estimate cluster masses and velocity dispersions for 123 clusters from optical spectroscopy to compare the Sunyaev-Zeldovich (SZ) mass proxy and dynamical masses. Our new survey, HeCS-SZ (Hectospec Cluster Survey of SZ-selected clusters), includes 7721 new or remeasured redshifts from MMT/Hectospec observations of 21 SZ-selected clusters at redshifts z = 0.05-0.20. We supplement the Hectospec data with spectra from the Sloan Digital Sky Survey (SDSS) and cluster data from the Cluster Infall Regions in SDSS project and the Hectospec Cluster Survey, our Hectospec survey of clusters selected by X-ray flux. We measure the scaling relation between velocity dispersion and SZ mass estimates from the integrated Compton parameter for an SZ-complete sample of 83 clusters. The observed relation agrees very well with a simple virial scaling from mass (based on SZ) to velocity dispersion. The SZ mass estimates (calibrated with hydrostatic X-ray mass estimates) are not significantly biased compared to dynamical mass estimates under the assumption of small velocity bias of galaxies compared to dark matter particles. Significant mass bias in SZ mass estimates could relieve tension between cosmological results from Planck SZ cluster counts and Planck CMB data. In principle, SZ mass bias and velocity bias of galaxies could conspire to yield good agreement, but the required velocity bias is sigma(galaxy) = 0.77 sigma(DM), outside the range of recent models of velocity bias in the literature. More likely, SZ mass bias and velocity bias are both small, and the tension between SZ cluster counts and CMB data requires another explanation.
C1 [Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
[Geller, Margaret J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Diaferio, Antonaldo] Univ Turin, Dipartimento Fis, Turin, Italy.
[Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 130722, South Korea.
RP Rines, KJ (reprint author), Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
EM kenneth.rines@wwu.edu
FU Smithsonian Institution; grant Progetti di Ateneo/CSP TO of the
University of Torino [Call2 2012 0011]; INFN grant InDark; PRIN of the
Italian Ministry of University and Research
FX We thank Jim Bartlett and Nabila Aghanim for advice on using the Planck
SZ catalogs. M.J.G. is supported by the Smithsonian Institution. A.D.
acknowledges support from the grant Progetti di Ateneo/CSP TO Call2 2012
0011 "Marco Polo" of the University of Torino, the INFN grant InDark,
the grant PRIN 2012 "Fisica Astroparticellare Teorica" of the Italian
Ministry of University and Research. We thank Susan Tokarz for reducing
the spectroscopic data and Perry Berlind and Mike Calkins for assisting
with the observations. We also thank the telescope operators at the MMT
and Nelson Caldwell for scheduling Hectospec queue observations.
NR 89
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400063
ER
PT J
AU Wicks, RT
Alexander, RL
Stevens, M
Wilson, LB
Moya, PS
Vinas, A
Jian, LK
Roberts, DA
O'Modhrain, S
Gilbert, JA
Zurbuchen, TH
AF Wicks, R. T.
Alexander, R. L.
Stevens, M.
Wilson, L. B., III
Moya, P. S.
Vinas, A.
Jian, L. K.
Roberts, D. A.
O'Modhrain, S.
Gilbert, J. A.
Zurbuchen, T. H.
TI A PROTON-CYCLOTRON WAVE STORM GENERATED BY UNSTABLE PROTON DISTRIBUTION
FUNCTIONS IN THE SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; plasmas; solar wind; waves
ID MAGNETIC-FIELD; 1 AU; TEMPERATURE ANISOTROPY; SPECTRAL-ANALYSIS;
TURBULENCE; PLASMA; POWER; INSTABILITIES; STEREO; SUN
AB We use audification of 0.092 s cadence magnetometer data from the Wind spacecraft to identify waves with amplitudes >0.1 nT near. the ion gyrofrequency (similar to 0.1 Hz) with duration longer than 1 hr during 2008. We present one of the most common types of event for a case study and find it to be a proton-cyclotron wave storm, coinciding with highly radial magnetic field and a suprathermal proton beam close in density to the core distribution itself. Using linear Vlasov analysis, we conclude that the long-duration, large-amplitude waves are generated by the instability of the proton distribution function. The origin of the beam is unknown, but the radial field period is found in the trailing edge of a fast solar wind stream and resembles other events thought to be caused by magnetic field footpoint motion or interchange reconnection between coronal holes and closed field lines in the corona.
C1 [Wicks, R. T.] UCL, Mullard Space Sci Lab, Gower St, London WC1E 6BT, England.
[Alexander, R. L.; O'Modhrain, S.; Gilbert, J. A.; Zurbuchen, T. H.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Stevens, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Wilson, L. B., III; Jian, L. K.; Roberts, D. A.] NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20771 USA.
[Moya, P. S.; Vinas, A.] NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
[Moya, P. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Jian, L. K.] Univ Maryland, Dept Astron, GPHI, College Pk, MD 20742 USA.
RP Wicks, RT (reprint author), UCL, Mullard Space Sci Lab, Gower St, London WC1E 6BT, England.
EM r.wicks@ucl.ac.uk
RI Wicks, Robert/A-1180-2009; Jian, Lan/B-4053-2010; Moya,
Pablo/C-3163-2011; Wilson III, Lynn/D-4425-2012; Gilbert,
Jason/I-9020-2012
OI Wicks, Robert/0000-0002-0622-5302; Jian, Lan/0000-0002-6849-5527; Moya,
Pablo/0000-0002-9161-0888; Wilson III, Lynn/0000-0002-4313-1970;
Gilbert, Jason/0000-0002-3182-7014
FU NASA Postdoctoral Program at the Goddard Space Flight Center;
Conicyt-Becas Chile Postdoctoral Fellowship; Heliophysics Guest
Investigator grant; NASA [NNX13AI65G]
FX R.T.W. was supported by the NASA Postdoctoral Program at the Goddard
Space Flight Center, administered by Oak Ridge Associated Universities.
R.T.W. and D.A.R. acknowledge a Heliophysics Guest Investigator grant to
NASA GSFC for support P.S.M. thanks the Conicyt-Becas Chile Postdoctoral
Fellowship for financial support. L.K.J. was supported by NASA grant
NNX13AI65G. Wind data were obtained from the SPDF Web site
http://spdf.gsfc.nasa.gov. The authors thank L. Matteini for useful
discussions.
NR 42
TC 2
Z9 2
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 6
DI 10.3847/0004-637X/819/1/6
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400006
ER
PT J
AU Xu, R
Bai, XN
AF Xu, Rui
Bai, Xue-Ning
TI ON THE GRAIN-MODIFIED MAGNETIC DIFFUSIVITIES IN PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; magnetohydrodynamics (MHD); protoplanetary
disks
ID WIND-DRIVEN ACCRETION; MAGNETOROTATIONAL-INSTABILITY; PROTOSTELLAR
DISKS; NONLINEAR EVOLUTION; AMBIPOLAR DIFFUSION; LINEAR-ANALYSIS; OUTER
REGIONS; TURBULENCE; DISCS; IONIZATION
AB Weakly ionized protoplanetary disks (PPDs) are subject to nonideal magnetohydrodynamic (MHD) effects, including ohmic resistivity, the Hall effect, and ambipolar diffusion (AD), and the resulting magnetic diffusivities (eta(O), eta(H), and eta(A)) largely control the disk gas dynamics. The presence of grains not only strongly reduces the disk ionization fraction, but also modifies the scalings of eta(H) and eta(A) with magnetic field strength. We analytically derive asymptotic expressions of eta(H) and eta(A) in both the strong and weak field limits and show that toward a strong field, eta(H) can change sign (at a threshold field strength B-th), mimicking a flip of field polarity, and AD is substantially reduced. Applied to PPDs, we find that when small similar to 0.1 (0.01) mu m grains are sufficiently abundant (mass ratio similar to 0.01 (10(-4))), eta(H) can change sign up to similar to 2-3 scale heights above the midplane at a modest field strength (plasma beta similar to 100) over a wide range of disk radii. The reduction of AD is also substantial toward the AD-dominated outer disk and may activate the magnetorotational instability. We further perform local nonideal MHD simulations of the inner disk (within 10 au) and show that, with sufficiently abundant small grains, the magnetic field amplification due to the Hall-shear instability saturates at a very low level near the threshold field strength B-th. Together with previous studies, we conclude by discussing the grainabundance- dependent phenomenology of PPD gas dynamics.
C1 [Xu, Rui] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Xu, Rui] Peking Univ, Yuanpei Coll, Beijing 100871, Peoples R China.
[Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA.
RP Xu, R (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.; Xu, R (reprint author), Peking Univ, Yuanpei Coll, Beijing 100871, Peoples R China.; Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA.
EM ruix@princeton.edu; xbai@cfa.harvard.edu
FU Institute for Theory and Computation (ITC) at the Harvard-Smithsonian
Center for Astrophysics
FX We thank the Institute for Advanced Study at Tsinghua University
(IASTU), Beijing, China, for hosting the spring school on planet
formation in 2014 May, where this project was initiated, and we thank
Doug Lin and Dong Lai for their initiatives in organizing the spring
school. We thank K. Oberg for helpful advice on disk chemistry and an
anonymous referee for useful suggestions. X.N.B. acknowledges support
from the Institute for Theory and Computation (ITC) at the
Harvard-Smithsonian Center for Astrophysics.
NR 40
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2016
VL 819
IS 1
AR 68
DI 10.3847/0004-637X/819/1/68
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZY
UT WOS:000372303400068
ER
PT J
AU Tellez, P
Rojas, E
Van Bael, S
AF Tellez, Peter
Rojas, Enith
Van Bael, Sunshine
TI Red coloration in young tropical leaves associated with reduced fungal
pathogen damage
SO BIOTROPICA
LA English
DT Article
DE anthocyanins; Calonectria sp; canopy crane system; Panama; tropical wet
forest
ID RAIN-FOREST; ANTHOCYANINS; PHOTODAMAGE; FLAVONOIDS; HERBIVORES;
PROTECTION
AB The adaptive significance of red coloration in tropical forest leaves remains unclear. In vivo assays show that there is a significant negative correlation between anthocyanin pigments in young leaves and fungal pathogen damage. This supports a previous hypothesis that anthocyanins may protect young leaves from fungal damage during the vulnerable period of leaf expansion.
Resumen El significado adaptativo de coloracion roja en las hojas de los bosques tropicales sigue siendo poco claro. Ensayos invivo muestran que existe una correlacion negativa significativa entre los pigmentos de antocianina en hojas jovenes rojas y danos por un hongo patogeno. Esto sugiere que las antocianinas pueden proteger a las hojas durante el periodo vulnerable de expansion.
C1 [Tellez, Peter; Van Bael, Sunshine] Tulane Univ, Dept Ecol & Evolutionary Biol, 6823 St Charles Ave, New Orleans, LA 70118 USA.
[Rojas, Enith; Van Bael, Sunshine] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
RP Van Bael, S (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, 6823 St Charles Ave, New Orleans, LA 70118 USA.; Van Bael, S (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
EM svanbael@tulane.edu
FU Smithsonian Tropical Research Institute (STRI); Tropical Canopy Biology
Program at STRI; Tulane University (The School of Science and
Engineering); Tulane University (Stone Center for Latin American
Studies); STRI; [NSF-DEB-0949602]
FX We thank Joe Wright, Mirna Samaniego, Emma Tower, Kimberly Mighell,
Gloribel Vergara Guerrero, and Elizabeth Kimbrough for their help and
for comments on early drafts. We thank the Smithsonian Tropical Research
Institute (STRI) and the Tropical Canopy Biology Program at STRI for
their support. Funding was from NSF-DEB-0949602 to SAV, Tulane
University (The School of Science and Engineering and the Stone Center
for Latin American Studies) and STRI.
NR 27
TC 1
Z9 1
U1 2
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0006-3606
EI 1744-7429
J9 BIOTROPICA
JI Biotropica
PD MAR
PY 2016
VL 48
IS 2
BP 150
EP 153
DI 10.1111/btp.12303
PG 4
WC Ecology
SC Environmental Sciences & Ecology
GA DH0YM
UT WOS:000372510600004
ER
PT J
AU Davis, M
Munoz, SP
AF Davis, Matt
Munoz, Silvia Pineda
TI The temporal scale of diet and dietary proxies
SO ECOLOGY AND EVOLUTION
LA English
DT Review
DE Diet; dietary proxies; isotopes; microwear; temporal scale; time
averaging
ID PLEISTOCENE GROUND SLOTHS; STABLE-ISOTOPE ANALYSES; DENTAL MICROWEAR;
LARGE HERBIVORES; CARBON-ISOTOPE; ANIMAL-TISSUES; NORTH-AMERICA;
GEOGRAPHIC-VARIATION; TOOTH MICROWEAR; AFRICAN BOVIDAE
AB Diets estimated from different proxies such as stable isotopes, stomach contents, and dental microwear often disagree, leading to nominally well-supported but greatly differing estimates of diet for both extinct and extant species that complicate our understanding of ecology. We show that these perceived incongruences can be caused by proxies recording diet over vastly different time-scales. Field observations reveal a diet averaged over minutes or hours, whereas dental morphology may reflect the diet of a lineage over millions of years of evolution. Failing to explicitly consider the scale of proxies and the potentially large temporal variability in diet can cause erroneous predictions in any downstream analyses such as conservation planning or paleohabitat reconstructions. We propose a cross-scale framework for conceptualizing diet suitable for both modern ecologists and paleontologists and provide recommendations for any studies involving dietary data. Treating diet in this temporally explicit framework and matching the scale of our questions with the scale of our data will lead to a much richer and clearer understanding of ecological and evolutionary processes.
C1 [Davis, Matt] Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA.
[Davis, Matt; Munoz, Silvia Pineda] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20004 USA.
RP Davis, M (reprint author), Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA.
EM matthew.davis@yale.edu
OI Pineda-Munoz, Silvia/0000-0003-0597-4456
FU Geological Society of America; American Society of Mammalogists; Yale
Institute for Biospheric Studies; International Palaeontological
Association and Congress; Macquarie University's HDR Project Support
Funds; Yale Peabody Museum Vertebrate Paleontology Fund; Smithsonian
Institution Predoctoral Fellowships; Terrestrial Ecosystems Program
publication [340]; [NSF-DEB 1257625]
FX Partial support for this research was provided by grants from the
Geological Society of America, the American Society of Mammalogists, the
Yale Institute for Biospheric Studies, the International
Palaeontological Association and Congress, Macquarie University's HDR
Project Support Funds, the Yale Peabody Museum Vertebrate Paleontology
Fund, two Smithsonian Institution Predoctoral Fellowships, and NSF-DEB
1257625. This is Evolution of Terrestrial Ecosystems Program publication
340.
NR 119
TC 4
Z9 4
U1 4
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD MAR
PY 2016
VL 6
IS 6
BP 1883
EP 1897
DI 10.1002/ece3.2054
PG 15
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DH0QI
UT WOS:000372488300026
PM 27087936
ER
PT J
AU Redmond, LJ
Murphy, MT
Cooper, NW
O'Reilly, KM
AF Redmond, Lucas J.
Murphy, Michael T.
Cooper, Nathan W.
O'Reilly, Kathleen M.
TI Testosterone secretion in a socially monogamous but sexually promiscuous
migratory passerine
SO GENERAL AND COMPARATIVE ENDOCRINOLOGY
LA English
DT Article
DE Androgens; Hormones; Kingbirds; Mating system; Testosterone; Tyrannus
ID DARK-EYED JUNCOS; MALE PARENTAL BEHAVIOR; RED-WINGED BLACKBIRDS;
EXTRA-PAIR PATERNITY; SUPERB FAIRY-WRENS; BLUE-HEADED VIREO; MALE GREAT
TITS; PLASMA TESTOSTERONE; EASTERN KINGBIRDS; REPRODUCTIVE SUCCESS
AB The steroid hormone testosterone (T) influences a multitude of traits critical to reproduction in vertebrates. In birds, high male T supports territory establishment and mate attraction, but is thought to interfere with parental care. Interspecific comparisons indicate that migratory species with short, synchronous breeding seasons have the highest peak T, and that the seasonal profile of T exhibits a rapid decline with the onset of incubation by females. We describe the T profile of the migratory, socially monogamous, and biparental Eastern Kingbird (Tyrannus tyrannus) from the high desert of eastern Oregon, USA, where breeding occurs within a short 2-3 month period. Eastern Kingbirds are socially monogamous but exhibit high rates of extra-pair paternity as similar to 60% of broods contain extra-pair young. We therefore evaluate whether Eastern Kingbirds exhibit the "typical" T profile expected for a synchronously breeding migratory species, or whether T is maintained at a more constant level as would be predicted for a species with opportunities for mating that extend over a majority of the breeding season. Our samples were divided into six periods of the reproductive cycle from territory establishment to the feeding of fledglings. T did not change across stages of the nest cycle. Instead, T declined with sampling date and nest density, and increased with the number of fertile females in the population. Male kingbirds advertise their presence through song for most of the breeding season, and we suggest that T is maintained throughout most of the breeding season because male fitness is equally dependent on within- and extra-pair reproductive success. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Redmond, Lucas J.; Murphy, Michael T.; Cooper, Nathan W.] Portland State Univ, Dept Biol, POB 751, Portland, OR 97201 USA.
[O'Reilly, Kathleen M.] Univ Portland, Dept Biol, 5000 N Willamette Blvd, Portland, OR 97203 USA.
[Cooper, Nathan W.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA.
RP Redmond, LJ (reprint author), Penn State Univ, Dept Biol, Schuylkill Campus,200 Univ Dr, Schuylkill Haven, PA 17972 USA.
EM ljr5322@psu.edu
OI Cooper, Nathan/0000-0002-4667-1542
FU National Science Foundation [IOB-0539370]; Association for the Study of
Animal Behaviour; Portland State University
FX We would like to thank C.M. Chutter, D. Youngblood and M. Paris for
assistance in the field. Richard Roy and all other personnel at Malheur
National Wildlife refuge were instrumental in granting access to the
refuge's kingbird population so that we could conduct our work. This
research was supported by a National Science Foundation grant
(IOB-0539370) awarded to M. T. M. and K. M. O., a research grant from
the Association for the Study of Animal Behaviour to N. W. C., and
Forbes-Lea Grants from Portland State University to both L.J.R. and
N.W.C.
NR 92
TC 0
Z9 0
U1 7
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0016-6480
EI 1095-6840
J9 GEN COMP ENDOCR
JI Gen. Comp. Endocrinol.
PD MAR 1
PY 2016
VL 228
BP 24
EP 32
DI 10.1016/j.ygcen.2016.01.012
PG 9
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA DH3IT
UT WOS:000372681400004
PM 26808965
ER
PT J
AU Sahley, CT
Cervantes, K
Salas, E
Paredes, D
Pacheco, V
Alonso, A
AF Sahley, Catherine Teresa
Cervantes, Klauss
Salas, Edith
Paredes, Diego
Pacheco, Victor
Alonso, Alfonso
TI Primary seed dispersal by a sigmodontine rodent assemblage in a Peruvian
montane forest
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE frugivory; Peru; rodents; seed dispersal; Sigmodontinae; tropical
montane forest
ID PALM ASTROCARYUM-STANDLEYANUM; TRIBE BRASSICEAE BRASSICACEAE; RATS
PROECHIMYS-SEMISPINOSUS; BRAZILIAN ATLANTIC FOREST; FRUIT-EATING BIRDS;
RAIN-FOREST; TREE SEEDS; TROPHIC RELATIONSHIPS; SMALL MAMMALS; EVOLUTION
AB We examined quantity and quality components of primary seed dispersal for an assemblage of sigmodontine rodents in ahigh-elevationmontane tropical forest in Peru. We collected faecal samples from 134individuals belonging to seven rodent species from the subfamily Sigmodontinae (Cricetidae) over a 2-y period. We conducted seed viability tests for seeds found in faecal samples. We identified seeds from eight plant families (Bromeliaceae, Annonaceae, Brassicaceae, Ericaceae, Melastomatacae, Myrtaceae, Rosaceae, Solanaceae), nine genera and 13 morphospecies. The most abundant seeds belonged to Gaultheria sp. 1 (46% of total) and Miconia sp. 1 (31% of total), while the most viable seeds belonged to Greigia sp. (84% viability) and Guatteria sp. (80% viability). We utilized relative rodent abundance, seed species diversity, seed abundance and seed viability per rodent species to calculate an index of rodent disperser effectiveness, and found that Thomasomys kalinowskii was the most effective disperser, followed by Akodon torques, Calomys sorellus, Thomasomys oreas, Oligoryzomys andinus and Microryzomys minutus. Plant genera dispersed by sigmodontine rodents overlappedmore with bird-and terrestrial-mammal-dispersed plants than with bat-dispersed plants. Future neotropical seed dispersal studies should consider small rodents as potential seed-dispersers, especially in tropical habitats where small-seeded, berry-forming shrubs and trees are present.
C1 [Sahley, Catherine Teresa] Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Andean & Marine Biodivers Monitoring & Assessment, 9099 Woodcrest Dr, Brecksville, OH 44141 USA.
[Cervantes, Klauss; Salas, Edith; Pacheco, Victor] Univ Nacl Mayor San Marcos, Dept Mastozool, Museo Hist Nat, Ave Arenales 1256, Lima 14, Peru.
[Paredes, Diego] Univ Nacl Mayor San Marcos, Dept Dicotiledoneas, Lab Florist, Museo Hist Nat, Ave Arenales 1256, Lima 14, Peru.
[Pacheco, Victor] Univ Nacl Mayor San Marcos, Inst Ciencias Biol Antonio Raimondi, Fac Ciencias Biol, Ave Venezuela S-N, Lima 1, Peru.
[Alonso, Alfonso] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, 110 Jefferson Dr SW,MRC 705, Washington, DC 20013 USA.
RP Sahley, CT (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Andean & Marine Biodivers Monitoring & Assessment, 9099 Woodcrest Dr, Brecksville, OH 44141 USA.
EM ctsahley@gmail.com
FU Smithsonian Institution; PERU LNG; Peru Biodiversity Program, Center for
Conservation and Sustainability, Smithsonian Conservation Biology
Institute [37]
FX We thank the government of Peru (Direccion General Forestal y de Fauna,
Ministerio de Agricultura) for granting us permits to conduct the study
(No. 440-2009-AG-DGFFS-DGEFFS, No. 344-2010-AG-DGFFS-DGEFFS, No.
144-2012-AG-DGFF-DGEFFS). We are indebted to Edgar Rengifo, Cecilia
Barriga, Maria Peralta, Oscar Centty, David Figueroa, Juan Tito and
Wendy Calderon for assistance in the field, and to Edith Arias, Pamela
Nina and Giovana Vadillo for assistance in the laboratory. Ornella Sissa
and Karim Ledesma provided logistical support. We thank the Smithsonian
Institution and PERU LNG for financial support. This is publication # 37
from the Peru Biodiversity Program, Center for Conservation and
Sustainability, Smithsonian Conservation Biology Institute.
NR 71
TC 1
Z9 1
U1 3
U2 7
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0266-4674
EI 1469-7831
J9 J TROP ECOL
JI J. Trop. Ecol.
PD MAR
PY 2016
VL 32
BP 125
EP 134
DI 10.1017/S0266467416000043
PN 2
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA DH1CR
UT WOS:000372522500004
ER
PT J
AU Thurman, TJ
Seymoure, BM
AF Thurman, T. J.
Seymoure, B. M.
TI A bird's eye view of two mimetic tropical butterflies: coloration
matches predator's sensitivity
SO JOURNAL OF ZOOLOGY
LA English
DT Article
DE avian visual models; Batesian mimicry; coloration; Mimoides; Heliconius;
JNDs; aposematism; UV vision
ID HELICONIUS BUTTERFLIES; BATESIAN MIMICRY; VISUAL PIGMENTS; EVOLUTION;
SIGNALS; PHOTORECEPTORS; ECOLOGY; PATTERN; VISION; BLUE
AB Unprofitable prey with conspicuous warning signals are often mimicked by other species, which then gain protection from predators. How closely two mimetic species resemble one another depends upon the visual perception of the signal receiver. However, most studies of mimetic coloration have been conducted using only the human visual system, which differs greatly from that of most animals. To better understand mimicry, we should study mimetic visual signals through the eyes of the intended receiver. Here, we use avian visual models to test predictions of putative Batesian mimicry in two Amazonian butterflies, Mimoides pausanias and Heliconius sara. We calculated Just Noticeable Differences (JNDs) and tetrahedral color volumes for 11 different patches: iridescent blue, yellow bars, red spots and black background. Several color patches were not visually discriminable for both avian visual systems (UV/VIS and V/VIS), and visual discrimination (i.e. degree of mimicry) of color patches depended upon the avian visual system. These two butterfly species are more mimetic when viewed by their likely avian predators, which have V/VIS vision. Therefore, this mimetic assemblage may have evolved to be more spectrally accurate in the non-UV wavelengths which their avian predators are able to see. However, while many color patches of the two species were modeled to be difficult to discriminate, most color patches were not perfect matches regardless of visual system, and several patches were very poor mimics. Through this study we demonstrate the importance of testing putative mimetic assemblages using known predator perceptual models and lay a foundation for behavioral studies to further test mimicry in H. sara and M. pausanius.
C1 [Thurman, T. J.] McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada.
[Thurman, T. J.] McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada.
[Seymoure, B. M.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
[Thurman, T. J.; Seymoure, B. M.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Seymoure, BM (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
EM brett.seymoure@gmail.com
NR 51
TC 0
Z9 0
U1 22
U2 43
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0952-8369
EI 1469-7998
J9 J ZOOL
JI J. Zool.
PD MAR
PY 2016
VL 298
IS 3
BP 159
EP 168
DI 10.1111/jzo.12305
PG 10
WC Zoology
SC Zoology
GA DG8UK
UT WOS:000372358900001
ER
PT J
AU Burrell, RB
Keppel, AG
Clark, VM
Breitburg, DL
AF Burrell, Rebecca B.
Keppel, Andrew G.
Clark, Virginia M.
Breitburg, Denise L.
TI An automated monitoring and control system for flow-through co-cycling
hypoxia and pH experiments
SO LIMNOLOGY AND OCEANOGRAPHY-METHODS
LA English
DT Article
ID OCEAN ACIDIFICATION; ESTUARINE WATERS; SEAWATER PH; OXYGEN; SATURATION;
CHEMISTRY; DYNAMICS; LARVAE
AB Acidification research has exploded in recent years, however, experiments testing effects of co-cycling hypoxia and pH on ecological and physiological processes are rare, despite the pervasiveness and potential importance of co-varying fluctuations in these parameters. Co-cycling dissolved oxygen (DO) and pH are difficult to precisely control, as gases used for manipulation influence both parameters. We successfully developed a LabVIEW (TM)-based system capable of monitoring and controlling co-varying DO and pH in raw seawater flow-through aquaria. Using feedback from Oxyguard DO probes and Honeywell ion sensitive field effect transistor Durafet pH sensors, our system controls ratios of nitrogen, oxygen, carbon dioxide, atmospheric air, and CO2-stripped air within a total gas flow rate through mass flow controllers, to achieve target co-cycling DO and pH values in five treatments. Our system performed well in two long-term experiments investigating effects of diel-cycling hypoxia and pH on eastern oyster (Crassostrea virginica) feeding, growth, fecundity, Perkinsus sp. (Dermo) infection dynamics and immune response. In our 2013 adult oyster experiment, the severe low DO treatment averaged only 0.04 mg L-1 higher than the 0.50 mg L-1 target, and the moderate hypoxia averaged only 0.05 mg L-1 higher than the 1.30 mg L-1 target over 48 d of cycles. Mean pH for the hypercapnia plateau was within 0.02 above the 7.00 target. In our 2013 spat experiment, daily minimum DO in the severe and moderate hypoxia treatments were both within 0.06 mg L-1 of the 0.50 and 1.3 mg L-1 targets, respectively; hypercapnia plateau pH values were within 0.01 of our 7.00 target.
C1 [Burrell, Rebecca B.; Keppel, Andrew G.; Clark, Virginia M.; Breitburg, Denise L.] Smithsonian Environm Res Ctr, Marine Ecol Lab, POB 28, Edgewater, MD 21037 USA.
[Keppel, Andrew G.; Clark, Virginia M.] Univ Maryland, Marine Estuarine & Environm Sci Program, College Pk, MD 20742 USA.
RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, Marine Ecol Lab, POB 28, Edgewater, MD 21037 USA.
EM breitburgd@si.edu
FU NOAA Center for Sponsored Coastal Ocean Research [NA10NOS4780138]; REU
[NSF-DBI 1156799]
FX We would like to gratefully acknowledge support from our funding agency
NOAA Center for Sponsored Coastal Ocean Research, Grant No.
NA10NOS4780138 (PIs: D. Breitburg, T. Targett, K. Rose, B. Michael and
H. Townsend) and REU funding from Grant No. NSF-DBI 1156799. We wish to
thank J. Jariwala for translating our theoretical logic into a
functional program, T. Targett, P. Grecay, K. Bogue, and P. McElhany for
their insights into their automated control systems, R. Bourdon and K.
Heggie for their hard work and invaluable assistance, J. Miklas and A.
Reynolds for help with titrations, H. Soulen and I. Fang for
contributing dissolved oxygen and pH data, and W. Miller and A. Dickson
for their help and guidance.
NR 43
TC 2
Z9 2
U1 4
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1541-5856
J9 LIMNOL OCEANOGR-METH
JI Limnol. Oceanogr. Meth.
PD MAR
PY 2016
VL 14
IS 3
BP 168
EP 185
DI 10.1002/lom3.10077
PG 18
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA DH3QQ
UT WOS:000372701900002
ER
PT J
AU Singh, RP
Shafeeque, CM
Sharma, SK
Singh, R
Mohan, J
Sastry, KVH
Saxena, VK
Azeez, PA
AF Singh, R. P.
Shafeeque, C. M.
Sharma, S. K.
Singh, R.
Mohan, J.
Sastry, K. V. H.
Saxena, V. K.
Azeez, P. A.
TI Chicken sperm transcriptome profiling by microarray analysis
SO GENOME
LA English
DT Article
DE fertility biomarker; sperm RNA; embryonic development; egg;
fertilization
ID MESSENGER-RNA; SPERMATOZOAL RNA; EJACULATED SPERMATOZOA; EMBRYO
DEVELOPMENT; GENE-EXPRESSION; FERTILE MEN; MOTILITY; INSIGHTS; CELLS
AB It has been confirmed that mammalian sperm contain thousands of functional RNAs, and some of them have vital roles in fertilization and early embryonic development. Therefore, we attempted to characterize transcriptome of the sperm of fertile chickens using microarray analysis. Spermatozoal RNA was pooled from 10 fertile males and used for RNA preparation. Prior to performing the microarray, RNA quality was assessed using a bioanalyzer, and gDNA and somatic cell RNA contamination was assessed by CD4 and PTPRC gene amplification. The chicken sperm transcriptome was cross-examined by analysing sperm and testes RNA on a 4 x 44K chicken array, and results were verified by RT-PCR. Microarray analysis identified 21 639 predominantly nuclear-encoded transcripts in chicken sperm. The majority (66.55%) of the sperm transcripts were shared with the testes, while surprisingly, 33.45% transcripts were detected (raw signal intensity greater than 50) only in the sperm and not in the testes. The greatest proportion of up-regulated transcripts were responsible for signal transduction (63.20%) followed by embryonic development (56.76%) and cell structure (56.25%). Of the 20 most abundant transcripts, 18 remain uncharacterized, whereas the least abundant genes were mostly associated with the ribosome. These findings lay a foundation for more detailed investigations on sperm RNAs in chickens to identify sperm-based biomarkers for fertility.
C1 [Singh, R. P.; Shafeeque, C. M.; Azeez, P. A.] Salim Ali Ctr Ornithol & Nat Hist, Avian Physiol & Genet Div, Coimbatore 641108, Tamil Nadu, India.
[Sharma, S. K.; Mohan, J.; Sastry, K. V. H.; Saxena, V. K.] Cent Avian Res Inst, Izatnagar 243122, Uttar Pradesh, India.
[Singh, R.] Indian Vet Res Inst, Izatnagar 243122, Uttar Pradesh, India.
[Singh, R. P.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
RP Singh, RP (reprint author), Salim Ali Ctr Ornithol & Nat Hist, Avian Physiol & Genet Div, Coimbatore 641108, Tamil Nadu, India.; Singh, RP (reprint author), Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
EM SinghRP@si.edu
OI Sharma, Sanjeev Kumar/0000-0002-3273-0708
FU Science and Engineering Research Board (SERB), Department of Science and
Technology, Government of India [SERB/FT/LS-147/2011]
FX This work was supported by the Science and Engineering Research Board
(SERB), Department of Science and Technology, Government of India
(SERB/FT/LS-147/2011). We thank Genotypic Technology Private Limited
Bangalore for the microarray processing and data analysis reported in
this publication.
NR 36
TC 0
Z9 0
U1 1
U2 5
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0831-2796
EI 1480-3321
J9 GENOME
JI Genome
PD MAR
PY 2016
VL 59
IS 3
BP 185
EP 196
DI 10.1139/gen-2015-0106
PG 12
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA DG6MN
UT WOS:000372199200005
PM 26868024
ER
PT J
AU Ramirez-Chaves, HE
Suarez-Castro, AF
Morales-Martinez, DM
Vallejo-Pareja, MC
AF Ramirez-Chaves, Hector E.
Suarez-Castro, Andres Felipe
Morales-Martinez, Darwin M.
Vallejo-Pareja, Maria Camila
TI Richness and distribution of porcupines (Erethizontidae: Coendou) from
Colombia
SO MAMMALIA
LA English
DT Article
DE Amazonas region; distribution; Hystricomorpha; morphology; range
extension
ID CONSERVATION; MAMMALS
AB In spite of previous reviews, there is still no consensus on the information associated to the richness of the genus Coendou in Colombia. To clarify some issues concerning the distribution and the taxonomic identity of the species of Coendou in the country, we reviewed specimens from five natural history collections. We introduce the first record of Coendou ichillus from the Orinoco river basin of the country, extending the distribution of the species by more than 600 km to the north from previous known localities in Ecuador and Peru. Additionally, we present new records of C. pruinosus and C. quichua from the Amazonia and inter-Andean valleys, respectively. Only one skull presents the diagnostic characters of C. bicolor; thus, previous records of this species for the country were based on misidentifications. Coendou is distributed in seven of the nine geographic provinces of Colombia. Coendou prehensilis was found in five provinces and is expected to be present in the Amazonia, whereas C. pruinosus was documented in three provinces (North Andean, Orinoco and Guyana). The rest of the species of Coendou were distributed in one or two provinces. The richest provinces were North Andean and Orinoco with six and four Coendou species, respectively. The elevational ranges of C. prehensilis and C. pruinosus are revised to 0-1975 and 90-2200 m, respectively.
C1 [Ramirez-Chaves, Hector E.] Univ Queensland, Sch Biol Sci, Weisbecker Lab, Goddard Bldg 8, St Lucia, Qld 4072, Australia.
[Suarez-Castro, Andres Felipe] Univ Queensland, Sch Geog Planning & Environm Management, Rhodes Conservat Lab, Steele Bldg 3, St Lucia, Qld 4072, Australia.
[Morales-Martinez, Darwin M.] Univ Nacl Colombia, Grp Mastozool, Carrera 45 26-85, Bogota, Colombia.
[Morales-Martinez, Darwin M.] Univ Nacl Colombia, Inst Ciencias Nat, Carrera 45 26-85, Bogota, Colombia.
[Vallejo-Pareja, Maria Camila] Smithsonian Trop Res Inst, POB 0843-03092, Panama City, Panama.
RP Ramirez-Chaves, HE (reprint author), Univ Queensland, Sch Biol Sci, Weisbecker Lab, Goddard Bldg 8, St Lucia, Qld 4072, Australia.
EM hera.chaves@gmail.com
RI Ramirez Chaves, Hector Emilio/B-2909-2016
OI Ramirez Chaves, Hector Emilio/0000-0002-2454-9482
FU UQI Scholarship of the University of Queensland; COLCIENCIAS PhD
Scholarships; UQCent Scholarship of the University of Queensland
FX We thank Hugo Lopez-Arevalo (ICN), Maria del Pilar Rivas Pava (MHNUC),
Michael Hiermeier (ZSM), Jose Gregorio Moreno and Martha Patricia
Ramirez (UIS), and Fabio Forero and Arturo Gonzalez (IAvH) for allowing
us to review specimens under their care. Robert S. Voss (AMNH) provided
important information and measurements of Coendou quichua from Colombia.
Juan P. Lopez-Ordonez provided photographs of one individual of C.
prehensilis from Guaviare, and Miguel Rodriguez-Posada provided
photographs of specimens at UV collections. Payal Bal reviewed an early
version of this work. MCVP thanks Carlos Jaramillo (STRI), Christine D.
Bacon (University of Gothenburg), Jorge Hernandez (UIS), and Manuel
Paez-Reyes for their support. This work was partially supported by the
UQCent and UQI Scholarships of the University of Queensland (to HER-C),
and COLCIEN-CIAS PhD Scholarships (to AFSC).
NR 20
TC 0
Z9 0
U1 0
U2 0
PU WALTER DE GRUYTER GMBH
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0025-1461
EI 1864-1547
J9 MAMMALIA
JI Mammalia
PD MAR
PY 2016
VL 80
IS 2
BP 181
EP 191
DI 10.1515/mammalia-2014-0158
PG 11
WC Zoology
SC Zoology
GA DG4DD
UT WOS:000372020000006
ER
PT J
AU Leasi, F
Andrade, SCD
Norenburg, J
AF Leasi, Francesca
da Silva Andrade, Sonia Cristina
Norenburg, Jon
TI At least some meiofaunal species are not everywhere. Indication of
geographic, ecological and geological barriers affecting the dispersion
of species of Ototyphlonemertes (Nemertea, Hoplonemertea)
SO MOLECULAR ECOLOGY
LA English
DT Article
DE biogeography; DNA taxonomy; genetic dispersal; meiofauna;
phylogeography; speciation
ID CRYPTIC DIVERSITY; DNA-SEQUENCES; PHYLOGENETIC INFERENCE;
BRACHIONUS-PLICATILIS; PARTITIONING SCHEMES; RIBOSOMAL DNA; MULTIPLE
LOCI; DELIMITATION; ROTIFERA; DIVERGENCE
AB Most meiofaunal species are known to have a broad distribution with no apparent barriers to their dispersion. However, different morphological and/or molecular methods supported patterns of diversity and distribution that may be different among taxa while also conflicting within the same group. We accurately assessed the patterns of geographic distribution in actual genetic species of a marine meiofaunal animal model: Ototyphlonemertes. Specimens were collected from several sites around Europe, Northern and Central America, Southern America, Pacific Islands and Asia. We sequenced regions of two mitochondrial and two nuclear genes. Using single-gene, a concatenated data set, multilocus approaches and different DNA taxonomy methods, we disentangled the actual diversity and the spatial structures of haplotypes and tested the possible correlation between genetic diversity and geographic distance. The results show (i) the importance of using several genes to uncover both diversity and highlight phylogeographic relationships among species and that (ii) independent genetic evolutionary entities have a narrower distribution than morphological species. Moreover, (iii) a Mantel test supported a positive correlation between genetic and geographical distance. By sampling from the two sides of Isthmus of Panama, we were additionally able to identify lineage divergence times that are concordant with vicariance mechanisms caused by the geological closure of the seaway across the Isthmus. We therefore propose that in addition to distance, other geological and ecological conditions are also barriers to the dispersion of and gene flow in marine meiofaunal organisms.
C1 [Leasi, Francesca; Norenburg, Jon] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, NMNH, POB 37012, Washington, DC 20013 USA.
[da Silva Andrade, Sonia Cristina] Univ Sao Paulo, Dept Genet & Biol, Evolut IB, BR-05508090 Sao Paulo, SP, Brazil.
RP Leasi, F (reprint author), Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, NMNH, POB 37012, Washington, DC 20013 USA.
EM leasif@si.edu
RI LEASI, FRANCESCA/E-4361-2017
FU CNPq (MCT-Brazil); FAPESP [05/56347]; FAEP [519/292]; JNL; Buck Genome
Initiative fellowship
FX This data set represents over 20 years of collecting, with many people
facilitating the field and laboratory work. We are grateful to
individuals at the following facilities: Laboratory of Analytical
Biology (LAB) at Smithsonian National Museum of Natural History
(Washington D.C.), Smithsonian Marine Station at Fort Pierce, Florida
(this represents contribution #### from SMSFP); the Smithsonian field
station at Carrie Boss Cay, Belize (this represents its CCRL
contribution ###), especially Klaus Rutzler and Mike Carpenter; the
Smithsonian laboratories at Bocas del Toro and at Naos, Panama,
especially Rachel Collin; Centro de Biologic Marinha da Universidade de
Sao Paulo, Brazil, especially Alvaro Esteves Migotto and Gustavo
Fonseca; Universidad de Oriente, Isla Margarita, Venezuela, especially
Juan Bolarios; Tjarno Marine Biological Laboratory, Sweden; Tropical
Biosphere Research Center Sesoko Station, Japan; Seto Marine Biological
Laboratory, Japan; Akkeshi Marine Station, Japan (with special thanks to
Hiroshi Kajihara for facilitating much of the collecting in Japan);
Kewalo Marine Laboratory and thwai'i Institute of Marine Biology,
especially Michael Hadfield; Richard B. Gump Moorea Field Station,
French Polynesia, especially Arthur Anker, Gustav Paulay, Chris Meyer;
and for providing microscopy facilities to a stranger: John Dolan at
Observatoire Oceanologique de Villefranche, and Jose Lino Costa at
Institute de Oceanografia, Lisbon, and to the many innkeepers who let
and even helped JLN set up microscopes and study worms in their
lodgings. Special thanks are extended to Herman Wirshing for providing
part of genetic data; to Alexei Chernyshev, Marco Curini-Galletti, Mats
Envall, Katharina forger, Hiroshi Kajihara and Svetlana Maslakova for
specimens from various places; to Alejandro Martinez Garcia and Katrine
Worsaae for hosting JLN at a workshop in Lanzarote, Canary Islands; and
to Maikon di Domenico for facilitating fieldwork, in Brazil. Diego
Fontaneto, an anonymous reviewer, and the editor Simon Creer greatly
improved a previous version of the manuscript. SCSA was supported by a
fellowship from CNPq (MCT-Brazil) and by FAPESP and FAEP grants 05/56347
and 519/292, respectively. FL was supported by JNL, and Buck Genome
Initiative fellowship. The authors thank Vera Nisaka Solferini.
NR 66
TC 0
Z9 1
U1 3
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0962-1083
EI 1365-294X
J9 MOL ECOL
JI Mol. Ecol.
PD MAR
PY 2016
VL 25
IS 6
BP 1381
EP 1397
DI 10.1111/mec.13568
PG 17
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA DG7GW
UT WOS:000372253800012
PM 26840255
ER
PT J
AU Stewart, AJ
Fender, RP
Broderick, JW
Hassall, TE
Munoz-Darias, T
Rowlinson, A
Swinbank, JD
Staley, TD
Molenaar, GJ
Scheers, B
Grobler, TL
Pietka, M
Heald, G
McKean, JP
Bell, ME
Bonafede, A
Breton, RP
Carbone, D
Cendes, Y
Clarke, AO
Corbel, S
de Gasperin, F
Eisloffel, J
Falcke, H
Ferrari, C
Griemeier, JM
Hardcastle, MJ
Heesen, V
Hessels, JWT
Horneffer, A
Iacobelli, M
Jonker, P
Karastergiou, A
Kokotanekov, G
Kondratiev, VI
Kuniyoshi, M
Law, CJ
van Leeuwen, J
Markoff, S
Miller-Jones, JCA
Mulcahy, D
Orru, E
Pandey-Pommier, M
Pratley, L
Rol, E
Rottgering, HJA
Scaife, AMM
Shulevski, A
Sobey, CA
Stappers, BW
Tasse, C
van der Horst, AJ
van Velzen, S
van Weeren, RJ
Wijers, RAMJ
Wijnands, R
Wise, M
Zarka, P
Alexov, A
Anderson, J
Asgekar, A
Avruch, IM
Bentum, MJ
Bernardi, G
Best, P
Breitling, F
Bruggen, M
Butcher, HR
Ciardi, B
Conway, JE
Corstanje, A
de Geus, E
Deller, A
Duscha, S
Frieswijk, W
Garrett, MA
Gunst, AW
van Haarlem, MP
Hoeft, M
Horandel, J
Juette, E
Kuper, G
Loose, M
Maat, P
McFadden, R
McKay-Bukowski, D
Moldon, J
Munk, H
Norden, MJ
Paas, H
Polatidis, AG
Schwarz, D
Sluman, J
Smirnov, O
Steinmetz, M
Thoudam, S
Toribio, MC
Vermeulen, R
Vocks, C
Wijnholds, SJ
Wucknitz, O
Yatawatta, S
AF Stewart, A. J.
Fender, R. P.
Broderick, J. W.
Hassall, T. E.
Munoz-Darias, T.
Rowlinson, A.
Swinbank, J. D.
Staley, T. D.
Molenaar, G. J.
Scheers, B.
Grobler, T. L.
Pietka, M.
Heald, G.
McKean, J. P.
Bell, M. E.
Bonafede, A.
Breton, R. P.
Carbone, D.
Cendes, Y.
Clarke, A. O.
Corbel, S.
de Gasperin, F.
Eisloeffel, J.
Falcke, H.
Ferrari, C.
Griemeier, J. -M.
Hardcastle, M. J.
Heesen, V.
Hessels, J. W. T.
Horneffer, A.
Iacobelli, M.
Jonker, P.
Karastergiou, A.
Kokotanekov, G.
Kondratiev, V. I.
Kuniyoshi, M.
Law, C. J.
van Leeuwen, J.
Markoff, S.
Miller-Jones, J. C. A.
Mulcahy, D.
Orru, E.
Pandey-Pommier, M.
Pratley, L.
Rol, E.
Rottgering, H. J. A.
Scaife, A. M. M.
Shulevski, A.
Sobey, C. A.
Stappers, B. W.
Tasse, C.
van der Horst, A. J.
van Velzen, S.
van Weeren, R. J.
Wijers, R. A. M. J.
Wijnands, R.
Wise, M.
Zarka, P.
Alexov, A.
Anderson, J.
Asgekar, A.
Avruch, I. M.
Bentum, M. J.
Bernardi, G.
Best, P.
Breitling, F.
Bruggen, M.
Butcher, H. R.
Ciardi, B.
Conway, J. E.
Corstanje, A.
de Geus, E.
Deller, A.
Duscha, S.
Frieswijk, W.
Garrett, M. A.
Gunst, A. W.
van Haarlem, M. P.
Hoeft, M.
Horandel, J.
Juette, E.
Kuper, G.
Loose, M.
Maat, P.
McFadden, R.
McKay-Bukowski, D.
Moldon, J.
Munk, H.
Norden, M. J.
Paas, H.
Polatidis, A. G.
Schwarz, D.
Sluman, J.
Smirnov, O.
Steinmetz, M.
Thoudam, S.
Toribio, M. C.
Vermeulen, R.
Vocks, C.
Wijnholds, S. J.
Wucknitz, O.
Yatawatta, S.
TI LOFAR MSSS: detection of a low-frequency radio transient in 400 h of
monitoring of the North Celestial Pole
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: interferometers; techniques: image processing; radio
continuum: general
ID SOLAR-TYPE STARS; GAMMA-RAY BURST; SKY SURVEY; GALACTIC-CENTER;
NEUTRON-STARS; FLARE STARS; LARGE ARRAY; WIDE-FIELD; COSMOLOGICAL
DISTANCES; REIONIZATION WINDOWS
AB We present the results of a four-month campaign searching for low-frequency radio transients near the North Celestial Pole with the Low-Frequency Array (LOFAR), as part of the Multifrequency Snapshot Sky Survey (MSSS). The data were recorded between 2011 December and 2012 April and comprised 2149 11-min snapshots, each covering 175 deg(2). We have found one convincing candidate astrophysical transient, with a duration of a few minutes and a flux density at 60 MHz of 15-25 Jy. The transient does not repeat and has no obvious optical or high-energy counterpart, as a result of which its nature is unclear. The detection of this event implies a transient rate at 60 MHz of 3.9(-3.7)(+14.7) x 10(-4) d(-1) deg(-2), and a transient surface density of 1.5 x 10(-5) deg(-2), at a 7.9-Jy limiting flux density and similar to 10-min time-scale. The campaign data were also searched for transients at a range of other time-scales, from 0.5 to 297 min, which allowed us to place a range of limits on transient rates at 60MHz as a function of observation duration.
C1 [Stewart, A. J.; Fender, R. P.; Broderick, J. W.; Hassall, T. E.; Munoz-Darias, T.; Staley, T. D.; Pietka, M.; Karastergiou, A.] Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Stewart, A. J.; Fender, R. P.; Broderick, J. W.; Hassall, T. E.; Munoz-Darias, T.; Staley, T. D.; Pietka, M.; Breton, R. P.; Clarke, A. O.; Heesen, V.; Mulcahy, D.] Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Broderick, J. W.; Rowlinson, A.; Heald, G.; McKean, J. P.; Falcke, H.; Hessels, J. W. T.; Iacobelli, M.; Kondratiev, V. I.; van Leeuwen, J.; Orru, E.; Sobey, C. A.; Wise, M.; Asgekar, A.; Bentum, M. J.; de Geus, E.; Deller, A.; Duscha, S.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; van Haarlem, M. P.; Kuper, G.; Loose, M.; Maat, P.; McFadden, R.; Moldon, J.; Munk, H.; Norden, M. J.; Polatidis, A. G.; Sluman, J.; Toribio, M. C.; Vermeulen, R.; Wijnholds, S. J.; Yatawatta, S.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Munoz-Darias, T.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Munoz-Darias, T.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Rowlinson, A.; Swinbank, J. D.; Molenaar, G. J.; Scheers, B.; Carbone, D.; Cendes, Y.; Hessels, J. W. T.; Kokotanekov, G.; van Leeuwen, J.; Markoff, S.; Wijers, R. A. M. J.; Wijnands, R.; Wise, M.] Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Swinbank, J. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Molenaar, G. J.; Grobler, T. L.; Tasse, C.; Smirnov, O.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Scheers, B.] Ctr Wiskunde & Informat, Sci Pk 123, NL-1098 XG Amsterdam, Netherlands.
[Grobler, T. L.; Tasse, C.; Smirnov, O.] SKA South Africa, 3rd Floor,The Pk,Pk Rd, ZA-7405 Cape Town, South Africa.
[Heald, G.; McKean, J. P.; Shulevski, A.; Avruch, I. M.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Bell, M. E.] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
[Bell, M. E.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia.
[Bonafede, A.; de Gasperin, F.; Bruggen, M.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Breton, R. P.; Clarke, A. O.; Mulcahy, D.; Scaife, A. M. M.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Corbel, S.] Univ Paris Diderot, Lab AIM, CEA, IRFU,CNRS,INSU,CEA DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Corbel, S.; Griemeier, J. -M.; Zarka, P.] Univ Orleans, PSL Res Univ, Observ Paris, Stn Radioastron Nancay,OSUC, F-18330 Nancay, France.
[Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany.
[Falcke, H.; Jonker, P.; van Velzen, S.; Corstanje, A.; Horandel, J.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Ferrari, C.] Univ Nice Sophia Antipolis, UMR 7293, Lab Lagrange, CNRS,Observ Cote Azur, F-06300 Nice, France.
[Griemeier, J. -M.] Univ Orleans, CNRS, LPC2E, 3A,Ave Rech Sci, F-45071 Orleans 2, France.
[Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Horneffer, A.; Wucknitz, O.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Jonker, P.; Avruch, I. M.] SRON Netherlands Insitute Space Res, POB 800, NL-9700 AV Groningen, Netherlands.
[Kondratiev, V. I.] Lebedev Phys Inst, Astro Space Ctr, Profsoyuznaya Str 84-32, Moscow 117997, Russia.
[Kuniyoshi, M.] Natl Astron Observ Japan, NAOJ Chile Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Law, C. J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Law, C. J.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Av Charles Andr E, F-69561 St Genis Laval, France.
[Pratley, L.] Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand.
[Rol, E.] Monash Univ, Sch Phys & Astron, POB 27, Clayton, Vic 3800, Australia.
[Rottgering, H. J. A.; Garrett, M. A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France.
[van der Horst, A. J.] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
[van Weeren, R. J.; Bernardi, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Zarka, P.] Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESLA, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Alexov, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Dept Geodesy & Remote Sensing 1, Helmholtz Zentrum Potsdam, Telegrafenberg A17, D-14473 Potsdam, Germany.
[Asgekar, A.] Shell Technol Ctr, Bangalore, Karnataka, India.
[Bentum, M. J.] Univ Twente, POB 217, NL-7500 AE Enschede, Netherlands.
[Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Breitling, F.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Via Cotter Rd, Weston, ACT 2611, Australia.
[Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden.
[de Geus, E.] SmarterVis BV, Oostersingel 5, NL-9401 JX Assen, Netherlands.
[Juette, E.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany.
[McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, FI-99600 Sodankyla, Finland.
[McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England.
[Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands.
[Schwarz, D.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany.
RP Stewart, AJ (reprint author), Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England.; Stewart, AJ (reprint author), Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM adam.stewart@physics.ox.ac.uk
RI Miller-Jones, James/B-2411-2013; Kondratiev, Vladislav/N-1105-2015;
Breton, Rene/A-5536-2017; Yatawatta, Sarod/E-6037-2013;
OI Hardcastle, Martin/0000-0003-4223-1117; Miller-Jones,
James/0000-0003-3124-2814; Shulevski, Aleksandar/0000-0002-1827-0469;
Kondratiev, Vladislav/0000-0001-8864-7471; Breton,
Rene/0000-0001-8522-4983; Wijers, Ralph/0000-0002-3101-1808; Staley,
Tim/0000-0002-4474-5253; Yatawatta, Sarod/0000-0001-5619-4017; Deller,
Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660
FU European Research Council [267697 4, 247295]; Spanish Ministerio de
Economia y competitividad (MINECO) [AYA2013-42627]; Netherlands eScience
Center; South African Research Chairs Initiative of the Department of
Science and Technology; National Research Foundation; UnivEarthS Labex
program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02];
NWO; European Research Council under the European Union / ERC [337062];
UK Science and Technology Facilities Council
FX A.J.S., J.W.B., T.E.H., T.M.-D., T.D.S. and M.P. acknowledge support
from the European Research Council via Advanced Investigator Grant no.
267697 4 Pi Sky: Extreme Astrophysics with Revolutionary Radio
Telescopes (PI: R.P. Fender). T.M.-D. also acknowledges support by the
Spanish Ministerio de Economia y competitividad (MINECO) under grant
AYA2013-42627. A.R., J.D.S., G.J.M., D.C., Y.C. and A.J.vdH. acknowledge
support from the European Research Council via Advanced Investigator
Grant no. 247295 (PI: R.A.M.J. Wijers). B.S. acknowlegdes partial
funding from the research programme of the Netherlands eScience Center
(www.nlesc.nl). T.L.G. acknowledges support from the South African
Research Chairs Initiative of the Department of Science and Technology
and National Research Foundation. S.C. acknowledges financial support
from the UnivEarthS Labex program of Sorbonne Paris Cite
(ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). J.W.T.H. acknowledges
funding from an NWO Vidi fellowship and from the European Research
Council under the European Union's Seventh Framework Programme
(FP/2007-2013) / ERC Starting Grant agreement nr. 337062 ('DRAGNET").r
The LT is operated on the island of La Palma by Liverpool John Moores
University in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias with financial support from the UK
Science and Technology Facilities Council.
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2016
VL 456
IS 3
BP 2321
EP 2342
DI 10.1093/mnras/stv2797
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LG
UT WOS:000372265200004
ER
PT J
AU Giannantonio, T
Fosalba, P
Cawthon, R
Omori, Y
Crocce, M
Elsner, F
Leistedt, B
Dodelson, S
Benoit-Levy, A
Gaztanaga, E
Holder, G
Peiris, HV
Percival, WJ
Kirk, D
Bauer, AH
Benson, BA
Bernstein, GM
Carretero, J
Crawford, TM
Crittenden, R
Huterer, D
Jain, B
Krause, E
Reichardt, CL
Ross, AJ
Simard, G
Soergel, B
Stark, A
Story, KT
Vieira, JD
Weller, J
Abbott, T
Abdalla, FB
Allam, S
Armstrong, R
Banerji, M
Bernstein, RA
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Capozzi, D
Carlstrom, JE
Rosell, AC
Kind, MC
Castander, FJ
Chang, CL
Cunha, CE
da Costa, LN
D'Andrea, CB
DePoy, DL
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Eifler, TF
Evrard, AE
Neto, AF
Fernandez, E
Finley, DA
Flaugher, B
Frieman, J
Gerdes, D
Gruen, D
Gruendl, RA
Gutierrez, G
Holzapfel, WL
Honscheid, K
James, DJ
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Lima, M
March, M
Marshall, JL
Martini, P
Melchior, P
Miquel, R
Mohr, JJ
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Romer, AK
Roodman, A
Rykoff, ES
Sako, M
Saliwanchik, BR
Sanchez, E
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Vikram, V
Walker, AR
Wechsler, RH
Zuntz, J
AF Giannantonio, T.
Fosalba, P.
Cawthon, R.
Omori, Y.
Crocce, M.
Elsner, F.
Leistedt, B.
Dodelson, S.
Benoit-Levy, A.
Gaztanaga, E.
Holder, G.
Peiris, H. V.
Percival, W. J.
Kirk, D.
Bauer, A. H.
Benson, B. A.
Bernstein, G. M.
Carretero, J.
Crawford, T. M.
Crittenden, R.
Huterer, D.
Jain, B.
Krause, E.
Reichardt, C. L.
Ross, A. J.
Simard, G.
Soergel, B.
Stark, A.
Story, K. T.
Vieira, J. D.
Weller, J.
Abbott, T.
Abdalla, F. B.
Allam, S.
Armstrong, R.
Banerji, M.
Bernstein, R. A.
Bertin, E.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Capozzi, D.
Carlstrom, J. E.
Rosell, A. Carnero
Kind, M. Carrasco
Castander, F. J.
Chang, C. L.
Cunha, C. E.
da Costa, L. N.
D'Andrea, C. B.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Eifler, T. F.
Evrard, A. E.
Fausti Neto, A.
Fernandez, E.
Finley, D. A.
Flaugher, B.
Frieman, J.
Gerdes, D.
Gruen, D.
Gruendl, R. A.
Gutierrez, G.
Holzapfel, W. L.
Honscheid, K.
James, D. J.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Lima, M.
March, M.
Marshall, J. L.
Martini, P.
Melchior, P.
Miquel, R.
Mohr, J. J.
Nichol, R. C.
Nord, B.
Ogando, R.
Plazas, A. A.
Romer, A. K.
Roodman, A.
Rykoff, E. S.
Sako, M.
Saliwanchik, B. R.
Sanchez, E.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Vikram, V.
Walker, A. R.
Wechsler, R. H.
Zuntz, J.
TI CMB lensing tomography with the DES Science Verification galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmic background radiation; gravitational lensing: weak; large-scale
structure of Universe
ID DIGITAL SKY SURVEY; LARGE-SCALE STRUCTURE; MICROWAVE BACKGROUND
ANISOTROPIES; INTEGRATED SACHS-WOLFE; SOUTH-POLE TELESCOPE; CHALLENGE
LIGHTCONE SIMULATION; ATACAMA COSMOLOGY TELESCOPE; PRIMORDIAL
NON-GAUSSIANITY; ANGULAR POWER SPECTRUM; DARK ENERGY SURVEY
AB We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 < z(phot) < 1.2, a cross-correlation signal is detected at 6 sigma and 4 sigma with SPT and Planck, respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant (>2 sigma) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z < 1.2 universe is 0.73 +/- 0.16 times as large as predicted in the Lambda cold dark matter Planck cosmology, a 1.7 sigma deviation.
C1 [Giannantonio, T.; Soergel, B.; Banerji, M.] Univ Cambridge, Inst Astron, Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England.
[Giannantonio, T.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England.
[Giannantonio, T.; Weller, J.; Desai, S.; Dietrich, J. P.; Gruen, D.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany.
[Fosalba, P.; Crocce, M.; Gaztanaga, E.; Bauer, A. H.; Carretero, J.] Campus UAB, Fac Ciencies, IEEC CSIC, Inst Ciencies Espai, Torre C5 Par 2, E-08193 Barcelona, Spain.
[Cawthon, R.; Dodelson, S.; Benson, B. A.; Crawford, T. M.; Carlstrom, J. E.; Chang, C. L.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Cawthon, R.; Dodelson, S.; Benson, B. A.; Story, K. T.; Carlstrom, J. E.; Chang, C. L.] Kavli Inst Cosmol Phys, 933 East 56th St, Chicago, IL 60637 USA.
[Omori, Y.; Holder, G.; Simard, G.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
[Elsner, F.; Leistedt, B.; Benoit-Levy, A.; Peiris, H. V.; Kirk, D.; Lahav, O.] UCL, Dept Phys & Astron, Astrophys Grp, 132 Hampstead Rd, London NW1 2PS, England.
[Dodelson, S.; Benson, B. A.; Buckley-Geer, E.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Percival, W. J.; Crittenden, R.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England.
[Bernstein, G. M.; Jain, B.; Eifler, T. F.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
[Huterer, D.; Evrard, A. E.; Gerdes, D.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Krause, E.; Cunha, C. E.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Phys Astrophys Bldg,452 Lomita Mall, Stanford, CA 94305 USA.
[Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Ross, A. J.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA.
[Stark, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 12, Cambridge, MA 02138 USA.
[Story, K. T.; Carlstrom, J. E.] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Vieira, J. D.; Gruendl, R. A.] Univ Illinois, Dept Astron, MC 221,1002 West Green St, Urbana, IL 61801 USA.
[Weller, J.; Desai, S.; Dietrich, J. P.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Munich, Germany.
[Weller, J.; Gruen, D.; Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Chang, C. L.; Vikram, V.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Burke, D. L.; Roodman, A.; Rykoff, E. S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Rosell, A. Carnero; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Ogando, R.] Lab Interinstituc E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Rosell, A. Carnero; da Costa, L. N.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Fernandez, E.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[James, D. J.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Martini, P.; Suchyta, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Saliwanchik, B. R.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Phys Dept, Cleveland, OH 44106 USA.
[Sanchez, E.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
RP Giannantonio, T (reprint author), Univ Cambridge, Inst Astron, Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England.; Giannantonio, T (reprint author), Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England.; Giannantonio, T (reprint author), Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany.; Fosalba, P (reprint author), Campus UAB, Fac Ciencies, IEEC CSIC, Inst Ciencies Espai, Torre C5 Par 2, E-08193 Barcelona, Spain.
EM t.giannantonio@ast.cam.ac.uk; fosalba@ice.cat
RI Lima, Marcos/E-8378-2010; Fosalba Vela, Pablo/I-5515-2016; Ogando,
Ricardo/A-1747-2010; Sobreira, Flavia/F-4168-2015; Gaztanaga,
Enrique/L-4894-2014;
OI Stark, Antony/0000-0002-2718-9996; Ogando, Ricardo/0000-0003-2120-1154;
Sobreira, Flavia/0000-0002-7822-0658; Gaztanaga,
Enrique/0000-0001-9632-0815; CRAWFORD, THOMAS/0000-0001-9000-5013;
Dietrich, Jorg/0000-0002-8134-9591; Weller, Jochen/0000-0002-8282-2010;
Carrasco Kind, Matias/0000-0002-4802-3194; Abdalla,
Filipe/0000-0003-2063-4345
FU Kavli Foundation; STFC [ST/L000636/1]; Excellence Cluster 'Universe' of
Garching, Germany; MareNostrum supercomputer [AECT-2008-1-0009,
2010-1-0007]; Port d'Informacio Cientifica; Cosmo-HUB portal; MINECO
[ESP2013-48274-C3-1-P]; European Research Council under the European
Union [306478-CosmicDawn, 240672, 291329, 306478]; University of
Melbourne; Australian Research Council [DP150103208]; US Department of
Energy; US National Science Foundation; Ministry of Science and
Education of Spain; Science and Technology Facilities Council of the
United Kingdom; Higher Education Funding Council for England; National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign; Kavli Institute of Cosmological Physics at the
University of Chicago; Center for Cosmology and Astro-Particle Physics
at the Ohio State University; Mitchell Institute for Fundamental Physics
and Astronomy at Texas AM University; Financiadora de Estudos e
Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do
Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche
Forschungsgemeinschaft; Collaborating Institutions in the DES; National
Science Foundation [AST-1138766]; Argonne National Laboratory;
University of California at Santa Cruz; University of Cambridge; Centro
de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid;
University of Chicago; University College London; DES-Brazil Consortium;
University of Edinburgh; Eidgenossische Technische Hochschule (ETH)
Zurich; Fermi National Accelerator Laboratory; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster
Universe; University of Michigan; National Optical Astronomy
Observatory; University of Nottingham; Ohio State University; University
of Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory; Stanford University; University of Sussex; Texas AM
University; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; NSF
Physics Frontier Center grant [PHY-0114422]; Gordon and Betty Moore
Foundation through Grant GBMF [947]
FX TG thanks Anthony Challinor and George Efstathiou for comments on a
draft version of this paper, and James Fergusson, Martin Kilbinger and
Ariel Sanchez for useful discussions. TG acknowledges support from the
Kavli Foundation, STFC grant ST/L000636/1, and from the Excellence
Cluster 'Universe' of Garching, Germany, as well as the Institut de
Ciencies de l'Espai, IEEC-CSIC, Universitat Autonoma de Barcelona, for
hospitality. PF acknowledges support from the MareNostrum supercomputer
(BSC-CNS, http://www.bsc.es), grants AECT-2008-1-0009 to 2010-1-0007,
Port d'Informacio Cientifica (http://www.pic.es), and the Cosmo-HUB
portal (cosmohub.pic.es), where the MICE simulations were run, stored,
and distributed, respectively. PF is funded by MINECO, project
ESP2013-48274-C3-1-P. FE, BL and HVP were partially supported by the
European Research Council under the European Union's Seventh Framework
Programme (PP7/2007-2013) /ERC grant agreement no. 306478-CosmicDawn. CR
acknowledges support from the University of Melbourne and from the
Australian Research Council's Discovery Projects scheme (DP150103208).r
Funding for the DES Projects has been provided by the US Department of
Energy, the US National Science Foundation, the Ministry of Science and
Education of Spain, the Science and Technology Facilities Council of the
United Kingdom, the Higher Education Funding Council for England, the
National Center for Supercomputing Applications at the University of
Illinois at Urbana-Champaign, the Kavli Institute of Cosmological
Physics at the University of Chicago, the Center for Cosmology and
Astro-Particle Physics at the Ohio State University, the Mitchell
Institute for Fundamental Physics and Astronomy at Texas A&M University,
Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia,
Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the
Collaborating Institutions in the DES. The DES data management system is
supported by the National Science Foundation under Grant Number
AST-1138766.r The Collaborating Institutions are Argonne National
Laboratory, the University of California at Santa Cruz, the University
of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the University of Edinburgh, the
Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National
Accelerator Laboratory, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat Munchen and the associated Excellence
Cluster Universe, the University of Michigan, the National Optical
Astronomy Observatory, the University of Nottingham, The Ohio State
University, the University of Pennsylvania, the University of
Portsmouth, SLAC National Accelerator Laboratory, Stanford University,
the University of Sussex, and Texas A&M University.r The DES
participants from Spanish institutions are partially supported by MINECO
under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de
Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results
has received funding from the European Research Council under the
European Union's Seventh Framework Programme (FP7/2007-2013) including
ERC grant agreements 240672, 291329, and 306478.; r The SPT programme is
supported by the National Science Foundation through grant PLR-1248097.
Partial support is also provided by the NSF Physics Frontier Center
grant PHY-0114422 to theKavli Institute of Cosmological Physics at the
University of Chicago, the Kavli Foundation, and the Gordon and Betty
Moore Foundation through Grant GBMF#947 to the University of Chicago.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2016
VL 456
IS 3
BP 3213
EP 3244
DI 10.1093/mnras/stv2678
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LG
UT WOS:000372265200072
ER
PT J
AU Benetti, S
Chugai, NN
Utrobin, VP
Cappellaro, E
Patat, F
Pastorello, A
Turatto, M
Cupani, G
Neuhauser, R
Caldwell, N
Pignata, G
Tomasella, L
AF Benetti, S.
Chugai, N. N.
Utrobin, V. P.
Cappellaro, E.
Patat, F.
Pastorello, A.
Turatto, M.
Cupani, G.
Neuhaeuser, R.
Caldwell, N.
Pignata, G.
Tomasella, L.
TI The spectacular evolution of Supernova 1996al over 15 yr: a low-energy
explosion of a stripped massive star in a highly structured environment
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; LUMINOUS BLUE VARIABLES; LIGHT CURVES;
AG-CARINAE; CIRCUMSTELLAR INTERACTION; STANDARD STARS; II SUPERNOVAE; HR
CARINAE; EMISSION; DISTANCE
AB Spectrophotometry of SN 1996al carried out throughout 15 yr is presented. The early photometry suggests that SN 1996al is a linear Type II supernova, with an absolute peak of M-V similar to -18.2 mag. Early spectra present broad asymmetric Balmer emissions, with superimposed narrow lines with P-Cygni profile, and He I features with asymmetric broad emission components. The analysis of the line profiles shows that the H and He broad components form in the same region of the ejecta. By day +142, the H alpha profile dramatically changes: the narrow P-Cygni profile disappears, and the H alpha is fitted by three emission components that will be detected over the remaining 15 yr of the supernova (SN) monitoring campaign. Instead, the He I emissions become progressively narrower and symmetric. A sudden increase in flux of all He I lines is observed between 300 and 600 d. Models show that the SN luminosity is sustained by the interaction of low-mass (similar to 1.15 M-circle dot) ejecta, expelled in a low kinetic energy (similar to 1.6 x 10(50) erg) explosion, with highly asymmetric circumstellar medium. The detection of H alpha emission in pre-explosion archive images suggests that the progenitor was most likely a massive star (similar to 25 M-circle dot ZAMS) that had lost a large fraction of its hydrogen envelope before explosion, and was hence embedded in a H-rich cocoon. The low-mass ejecta and modest kinetic energy of the explosion are explained with massive fallback of material into the compact remnant, a 7-8-M-circle dot black hole.
C1 [Benetti, S.; Cappellaro, E.; Pastorello, A.; Turatto, M.; Tomasella, L.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Chugai, N. N.] Russian Acad Sci, Inst Astron, Pyatnitskaya St 48, Moscow 119017, Russia.
[Utrobin, V. P.] Inst Theoret & Expt Phys, B Cheremushkinskaya St 25, Moscow 117218, Russia.
[Patat, F.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Cupani, G.] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy.
[Neuhaeuser, R.] Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany.
[Neuhaeuser, R.] Univ Sternwarte, FSU Jena, Schillergasschen 2-3, D-07745 Jena, Germany.
[Caldwell, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile.
[Pignata, G.] Millennium Inst Astrophys, Santiago, Chile.
RP Benetti, S; Cappellaro, E (reprint author), INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
EM stefano.benetti@oapd.inaf.it; enrico.cappellaro@oapd.inaf.it
FU PRIN-INAF project Transient Universe: unveiling new types of stellar
explosions with PESSTO; Russian Scientific Foundation [14-12-00203];
Program of RAS 'Explosions in Astrophysics'; Millennium Institute of
Astrophysics (MAS) of the Programa Iniciativa Cientifica Milenio del
Ministerio de Economia, Fomento y Turismo de Chile [IC120009]; National
Aeronautics and Space Administration
FX SB, MT and AP are partially supported by the PRIN-INAF 2014 project
Transient Universe: unveiling new types of stellar explosions with
PESSTO. VPU is supported by Russian Scientific Foundation grant
14-12-00203. NC thanks the Program of RAS 'Explosions in Astrophysics'
for financial support. GP acknowledge support provided by the Millennium
Institute of Astrophysics (MAS) through grant IC120009 of the Programa
Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y
Turismo de Chile.; This research has made use of the NASA/IPAC
Extragalactic Database (NED) which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. We have also made use of
the Lyon-Meudon Extragalactic Database (LEDA), supplied by the LEDA team
at the Centre de Recherche Astronomique de Lyon, Observatoire de Lyon.
NR 70
TC 2
Z9 2
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2016
VL 456
IS 3
BP 3296
EP 3317
DI 10.1093/mnras/stv2811
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LG
UT WOS:000372265200077
ER
PT J
AU Anton, SC
Potts, R
Aiello, LC
AF Anton, Susan C.
Potts, Richard
Aiello, Leslie C.
TI An integrated perspective on the origin and evolution of Homo
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Anton, Susan C.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA.
[Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
[Aiello, Leslie C.] Wenner Gren Fdn Anthropol Research, Anthropol, New York, NY USA.
NR 0
TC 0
Z9 0
U1 9
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 82
EP 82
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255200033
ER
PT J
AU Brennan, EJ
Hunt, DR
AF Brennan, Emily J.
Hunt, David R.
TI Sexual dimorphism of the proximal ulna: An evaluation of metric analyses
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Brennan, Emily J.] George Washington Univ, Anthropol, Washington, DC 20052 USA.
[Brennan, Emily J.; Hunt, David R.] Smithsonian Inst, Anthropol, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 102
EP 102
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255200114
ER
PT J
AU Carlson, KJ
Chirchir, H
Patel, BA
AF Carlson, Kristian J.
Chirchir, Habiba
Patel, Biren A.
TI Subchondral properties of the hominoid distal tibia: an indicator of
loading during habitually dorsiflexed ankle postures
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Carlson, Kristian J.] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2050 Johannesburg, South Africa.
[Carlson, Kristian J.] Univ Witwatersrand, Sch Geosci, ZA-2050 Johannesburg, South Africa.
[Carlson, Kristian J.] Indiana Univ, Dept Anthropol, Bloomington, IN 47405 USA.
[Chirchir, Habiba] Marshall Univ, Dept Biol Sci, Huntington, WV 25755 USA.
[Chirchir, Habiba] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA.
[Patel, Biren A.] Univ So Calif, Keck Sch Med, Dept Cell & Neurobiol, Los Angeles, CA 90089 USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 109
EP 109
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255201002
ER
PT J
AU Chirchir, H
Ruff, CB
AF Chirchir, Habiba
Ruff, Christopher B.
TI Trabecular bone density in recent modern humans
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Chirchir, Habiba] Marshall Univ, Biol Sci, Huntington, WV 25755 USA.
[Chirchir, Habiba] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA.
[Ruff, Christopher B.] Johns Hopkins Univ, Ctr Funct Anat & Evolut, Baltimore, MD 21218 USA.
NR 0
TC 0
Z9 0
U1 3
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 116
EP 116
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255201029
ER
PT J
AU Cunningham, AS
Hunt, DR
Coolidge, RH
AF Cunningham, Andreana S.
Hunt, David R.
Coolidge, Rhonda H.
TI Biocultural evidence through taphonomic observations in the Karluk
Salmon Cannery Chinese of Kodiak Island, Alaska
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Cunningham, Andreana S.] Univ Miami, Anthropol, Coral Gables, FL 33124 USA.
[Cunningham, Andreana S.; Hunt, David R.; Coolidge, Rhonda H.] Smithsonian Inst, Anthropol, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 1
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 125
EP 125
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255201067
ER
PT J
AU Kivell, TL
Deane, AS
Tocheri, MW
Orr, CM
Schmid, P
Hawks, J
Berger, LR
Churchill, SE
AF Kivell, Tracy L.
Deane, Andrew S.
Tocheri, Matthew W.
Orr, Caley M.
Schmid, Peter
Hawks, John
Berger, Lee R.
Churchill, Steven E.
TI Functional interpretation of the Homo naledi hand
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Kivell, Tracy L.] Univ Kent, Sch Anthropol & Conservat, Canterbury CT2 7NZ, Kent, England.
[Kivell, Tracy L.] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Leipzig, Germany.
[Kivell, Tracy L.; Deane, Andrew S.; Schmid, Peter; Hawks, John; Berger, Lee R.; Churchill, Steven E.] Univ Witwatersrand, Evolutionary Studies Inst, ZA-2050 Johannesburg, South Africa.
[Kivell, Tracy L.; Deane, Andrew S.; Schmid, Peter; Hawks, John; Berger, Lee R.; Churchill, Steven E.] Univ Witwatersrand, Ctr Excellence PalaeoSci, ZA-2050 Johannesburg, South Africa.
[Deane, Andrew S.] Univ Kentucky, Coll Med, Dept Anat & Neurobiol, Lexington, KY 40506 USA.
[Tocheri, Matthew W.] Lakehead Univ, Dept Anthropol, Thunder Bay, ON P7B 5E1, Canada.
[Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA.
[Orr, Caley M.] Univ Colorado, Sch Med, Dept Cell & Dev Biol, Boulder, CO 80309 USA.
[Schmid, Peter] Univ Zuerich, Anthropol Inst & Museum, Zurich, Switzerland.
[Hawks, John] Univ Wisconsin, Dept Anthropol, Madison, WI 53706 USA.
[Churchill, Steven E.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA.
NR 0
TC 0
Z9 0
U1 6
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 192
EP 192
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255201336
ER
PT J
AU O'Malley, RC
Murray, CM
Nockerts, RS
Power, ML
AF O'Malley, Robert C.
Murray, Carson M.
Nockerts, Rebecca S.
Power, Michael L.
TI Nutritional composition of plant foods consumed by the chimpanzees of
Gombe National Park, Tanzania
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [O'Malley, Robert C.; Murray, Carson M.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA.
[Nockerts, Rebecca S.] Univ Minnesota, Dept Anthropol, Minneapolis, MN 55455 USA.
[Power, Michael L.] Natl Zool Pk, Smithsonian Inst, Nutr Lab, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 243
EP 243
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255202033
ER
PT J
AU Roach, NT
Hatala, KG
Ostrofsky, KR
Villmoare, B
Reeves, JS
Du, A
Braun, DR
Harris, JW
Behrensmeyer, AK
Richmond, BG
AF Roach, Neil T.
Hatala, Kevin G.
Ostrofsky, Kelly R.
Villmoare, Brian
Reeves, Jonathan S.
Du, Andrew
Braun, David R.
Harris, John Wk.
Behrensmeyer, Anna K.
Richmond, Brian G.
TI Homo erectus paleoecology and behavior based on 1.5 million year old
footprints from northwestern Kenya
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Roach, Neil T.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA.
[Roach, Neil T.; Richmond, Brian G.] Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA.
[Hatala, Kevin G.] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, Leipzig, Germany.
[Hatala, Kevin G.; Ostrofsky, Kelly R.; Reeves, Jonathan S.; Du, Andrew; Braun, David R.] George Washington Univ, Ctr Adv Study Human Paleobiol, Washington, DC 20052 USA.
[Villmoare, Brian] Univ Nevada Las Vegas, Dept Anthropol, Las Vegas, NV USA.
[Harris, John Wk.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA.
[Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat History, Dept Paleobiol, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 2
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 270
EP 270
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255202140
ER
PT J
AU Romero, A
Sholts, S
Hakansson, H
Viluksela, M
AF Romero, Ashly
Sholts, Sabrina
Hakansson, Helen
Viluksela, Matti
TI Craniofacial and dental effects shown in rats following in
utero/lactational exposure to 2,2 ', 3,4,4 ', 5,5 '-heptachlorobiphenyl
(PCB-180)
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Romero, Ashly] Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA.
[Sholts, Sabrina] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA.
[Hakansson, Helen] Karolinska Inst, Inst Environm Med, S-10401 Stockholm, Sweden.
[Viluksela, Matti] Univ Eastern Finland, Dept Environm Sci, Joensuu, Finland.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 272
EP 272
PG 1
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255202148
ER
PT J
AU Sholts, SB
Huffman, M
Hlusko, LJ
AF Sholts, Sabrina B.
Huffman, Michaela
Hlusko, Leslea J.
TI Evolution of the Human Dentition: 5,000 years in the San Francisco Bay
Area
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Sholts, Sabrina B.] Smithsonian Inst, Nat Museum Nat Hist, Washington, DC 20560 USA.
[Huffman, Michaela; Hlusko, Leslea J.] Univ Calif Berkeley, Human Evolut Res Ctr, Berkeley, CA 94720 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 290
EP 291
PG 2
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255202223
ER
PT J
AU Smith-Guzman, NE
Rose, JC
Davis, HS
AF Smith-Guzman, Nicole E.
Rose, Jerome C.
Davis, Heidi S.
TI Malaria at Amarna, Egypt: Evidence from the South Tombs Cemetery
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Meeting Abstract
CT 85th Annual Meeting of the
American-Association-of-Physical-Anthropologists
CY APR 13-16, 2016
CL Atlanta, GA
SP Amer Assoc Phys Anthropologists
C1 [Smith-Guzman, Nicole E.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Panama City, Panama.
[Rose, Jerome C.; Davis, Heidi S.] Univ Arkansas, Dept Anthropol, Fayetteville, AR 72701 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
SU 62
BP 296
EP 297
PG 2
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF3OW
UT WOS:000371255202248
ER
PT J
AU Antoine, PO
Abello, MA
Adnet, S
Sierra, AJA
Baby, P
Billet, G
Boivin, M
Calderon, Y
Candela, A
Chabain, J
Corfu, F
Croft, DA
Ganerod, M
Jaramillo, C
Klaus, S
Marivaux, L
Navarrete, RE
Orliac, MJ
Parra, F
Perez, ME
Pujos, F
Rage, JC
Ravel, A
Robinet, C
Roddaz, M
Tejada-Lara, JV
Velez-Juarbe, J
Wesselingh, FP
Salas-Gismondi, R
AF Antoine, Pierre-Olivier
Alejandra Abello, M.
Adnet, Sylvain
Altamirano Sierra, Ali J.
Baby, Patrice
Billet, Guillaume
Boivin, Myriam
Calderon, Ysabel
Candela, Adriana
Chabain, Jules
Corfu, Fernando
Croft, Darin A.
Ganerod, Morgan
Jaramillo, Carlos
Klaus, Sebastian
Marivaux, Laurent
Navarrete, Rosa E.
Orliac, Maeva J.
Parra, Francisco
Encarnacion Perez, Maria
Pujos, Francois
Rage, Jean-Claude
Ravel, Anthony
Robinet, Celine
Roddaz, Martin
Victoria Tejada-Lara, Julia
Velez-Juarbe, Jorge
Wesselingh, Frank P.
Salas-Gismondi, Rodolfo
TI A 60-million-year Cenozoic history of western Amazonian ecosystems in
Contamana, eastern Peru
SO GONDWANA RESEARCH
LA English
DT Review
DE Fossil record; Paleobiology; Stratigraphy; Paleogeography; South America
ID MADRE-DE-DIOS; FORMATION LATE-MIOCENE; NEOTROPICAL RAIN-FOREST;
SUB-ANDEAN ZONE; SOUTH-AMERICA; MIDDLE MIOCENE; FORELAND BASIN; MARINE
INCURSIONS; CERREJON FORMATION; FOSSIL RECORD
AB We provide a synopsis of similar to 60 million years of life history in Neotropical lowlands, based on a comprehensive survey of the Cenozoic deposits along the Quebrada Cachiyacu near Contamana in Peruvian Amazonia. The 34 fossil bearing localities identified have yielded a diversity of fossil remains, including vertebrates, mollusks, arthropods, plant fossils, and microorganisms, ranging from the early Paleocene to the late Miocene-?Pliocene (>20 successive levels). This Cenozoic series includes the base of the Huchpayacu Formation (Fm.; early Paleocene; lacustrine/fluvial environments; charophyte-dominated assemblage), the Pozo Fm. (middle + ?late Eocene; marine then freshwater environments; most diversified biomes), and complete sections for the Chambira Fm. (late Oligocene-late early Miocene; freshwater environments; vertebrate-dominated faunas), the Pebas Fm. (late early to early late Miocene; freshwater environments with an increasing marine influence; excellent fossil record), and Ipururo Fm. (late Miocene-?Pliocene; fully fluvial environments; virtually no fossils preserved). At least 485 fossil species are recognized in the Contamana area (similar to 250 'plants', similar to 212 animals, and 23 foraminifera). Based on taxonomic lists from each stratigraphic interval, high-level taxonomic diversity remained fairly constant throughout the middle Eocene-Miocene interval (8-12 classes), ordinal diversity fluctuated to a greater degree, and family/species diversity generally declined, with a drastic drop in the early Miocene. The Paleocene-?Pliocene fossil assemblages from Contamana attest at least to four biogeographic histories inherited from (i) Mesozoic Gondwanan times, (ii) the Panamerican realm prior to (iii) the time of South America's Cenozoic "splendid isolation", and (iv) Neotropical ecosystems in the Americas. No direct evidence of any North American terrestrial immigrant has yet been recognized in the Miocene record at Contamana. (C) 2015 International Association for Gondwana Research. Published by Elsevier B.V. All rights reserved.
C1 [Antoine, Pierre-Olivier; Adnet, Sylvain; Boivin, Myriam; Chabain, Jules; Marivaux, Laurent; Orliac, Maeva J.; Ravel, Anthony; Robinet, Celine; Salas-Gismondi, Rodolfo] Univ Montpellier, EPHE, IRD, Inst Sci Evolut,UMR CNRS 5554, Pl Eugene Bataillon, F-34095 Montpellier 5, France.
[Alejandra Abello, M.] Museo La Plata, Lab Sistemat & Biol Evolut LASBE, Paseo Bosque S-N,B1900FWA, La Plata, Argentina.
[Alejandra Abello, M.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.
[Altamirano Sierra, Ali J.; Victoria Tejada-Lara, Julia; Salas-Gismondi, Rodolfo] Univ Nacl Mayor San Marcos, Museo Hist Nat, Dept Paleontol Vertebrados, Ave Arenales 1256, Lima 11, Peru.
[Baby, Patrice; Calderon, Ysabel; Parra, Francisco; Roddaz, Martin] Univ Toulouse, CNRS, LMTG, Geosci Environm Toulouse,UPS SVT OMP,IRD, 14 Ave Edouard Belin, F-31400 Toulouse, France.
[Baby, Patrice; Calderon, Ysabel] Convenio IRD PeruPetro, Av Luis Aldana 320, Lima, Peru.
[Billet, Guillaume; Rage, Jean-Claude] Univ Paris 06, Sorbonne Univ, CNRS, Museum Natl Hist Nat,MNHN,CR2P, CP 38,8 Rue Buffon, F-75231 Paris 05, France.
[Candela, Adriana; Robinet, Celine] Museo La Plata, Div Paleontol Vertebrados, Paseo Bosque S-N,B1900FWA, La Plata, Argentina.
[Corfu, Fernando] Univ Oslo, Dept Geosci, POB 1047 Blindem, NO-0316 Oslo, Norway.
[Croft, Darin A.] Case Western Reserve Univ, Sch Med, Dept Anat, Cleveland, OH 44106 USA.
[Ganerod, Morgan] Geol Survey Norway, N-7491 Trondheim, Norway.
[Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa 084303092, Ancon Aa, Panama.
[Klaus, Sebastian] Goethe Univ Frankfurt, Dept Ecol & Evolut, Max von Laue Str 13, D-60438 Frankfurt, Germany.
[Navarrete, Rosa E.; Parra, Francisco] Paleosedes EU, Tv 27 57-49 Campin, Bogota, Colombia.
[Encarnacion Perez, Maria] Consejo Nacl Invest Cient & Tecn, Museo Paleontol Egidio Feruglio, Av Fontana 140, Trelew, Argentina.
[Encarnacion Perez, Maria] Field Museum Nat Hist, 1400 Lake Shore Dr, Chicago, IL 60605 USA.
[Pujos, Francois] CCT CONICET Mendoza, IANIGLA, Ave Ruiz Leal S-N,Parque Gen San Martin, RA-5500 Mendoza, Argentina.
[Victoria Tejada-Lara, Julia] Columbia Univ, Lamont Doherty Earth Observ, Dept Earth & Environm Sci, Palisades, NY 10964 USA.
[Victoria Tejada-Lara, Julia] Amer Museum Nat Hist, Div Vertebrate Paleontol, New York, NY 10024 USA.
[Velez-Juarbe, Jorge] Nat Hist Museum Los Angeles Cty, Dept Mammal, Los Angeles, CA USA.
[Velez-Juarbe, Jorge] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
[Wesselingh, Frank P.] Nat Biodivers Ctr, POB 9517, NL-2300 RA Leiden, Netherlands.
RP Antoine, PO (reprint author), Univ Montpellier, EPHE, IRD, Inst Sci Evolut,UMR CNRS 5554, Pl Eugene Bataillon, F-34095 Montpellier 5, France.
EM pierre-olivier.antoine@umontpellier.fr
RI Roddaz, Martin/G-6894-2016
FU CNRS 'Eclipse 2' program; CNRS 'Paleo2' program; Toulouse University
'SPAM' program; PALASIAFRICA [ANR-08-JCJC-0017]; Alexander von
Humboldt-Foundation (Bonn); Agence Nationale de la Recherche (CEBA)
[ANR-10-LABX-25-01]
FX We are particularly grateful to the Canaan Shipibo Native Community and
Maple Gas Peru S.A. for granting access to the field, and to the
IRD-PeruPetro Convention Programme for logistic support. We thank warmly
our guides Manuel and Manuel, Joaquin Sanancino, their families, and
whoever helped us in the field and in the lab. This article is dedicated
to the memory of Eduardo "Aldo" Musacchio. This work was supported by
CNRS 'Eclipse 2', CNRS 'Paleo2', Toulouse University 'SPAM' programs, by
ANR-08-JCJC-0017 (PALASIAFRICA) program, by the Alexander von
Humboldt-Foundation (Bonn), and by an "Investissements d'Avenir" grant
managed by Agence Nationale de la Recherche (CEBA, ANR-10-LABX-25-01).
NR 195
TC 11
Z9 11
U1 3
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1342-937X
EI 1878-0571
J9 GONDWANA RES
JI Gondwana Res.
PD MAR
PY 2016
VL 31
BP 30
EP 59
DI 10.1016/j.gr.2015.11.001
PG 30
WC Geosciences, Multidisciplinary
SC Geology
GA DF7RK
UT WOS:000371555100003
ER
PT J
AU Wynn, AH
Diesmos, AC
Brown, RM
AF Wynn, Addison H.
Diesmos, Arvin C.
Brown, Rafe M.
TI Two New Species of Malayotyphlops from the Northern Philippines, with
Redescriptions of Malayotyphlops luzonensis (Taylor) and Malayotyphlops
ruber (Boettger)
SO JOURNAL OF HERPETOLOGY
LA English
DT Article
ID BLIND SNAKE; ISLAND; LUPEROSAURUS; TYPHLOPIDAE; ARCHIPELAGO; SERPENTES;
SQUAMATA
AB As a first step toward making sense of an infamously enigmatic and taxonomically problematic group of Philippine blind snakes, we redescribe Malayotyphlops luzonensis (Taylor, 1919) and Malayotyphlops ruber (Boettger, 1897) and clarify their taxonomic status with respect to each other and to additional phenotypically similar taxa. We also describe two other new species of Malayotyphlops from the Sierra Madre Mountain Range of northern Luzon Island, each on the basis of a single specimen. We suspect that species diversity of the typhlopid fauna of the Philippines is severely underestimated, with progress towards a comprehensive understanding of this group most hampered by a lack of sufficient comparative material available in biodiversity repositories.
C1 [Wynn, Addison H.] Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Diesmos, Arvin C.; Brown, Rafe M.] Philippine Natl Museum, Div Zool, Herpetol Sect, Rizal Pk,Pade Burgos St, Manila, Philippines.
[Diesmos, Arvin C.; Brown, Rafe M.] Univ Kansas, Biodivers Inst, Lawrence, KS 66045 USA.
[Diesmos, Arvin C.; Brown, Rafe M.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
RP Brown, RM (reprint author), Philippine Natl Museum, Div Zool, Herpetol Sect, Rizal Pk,Pade Burgos St, Manila, Philippines.; Brown, RM (reprint author), Univ Kansas, Biodivers Inst, Lawrence, KS 66045 USA.; Brown, RM (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
EM rafe@ku.edu
FU Rufford Foundation; National University of Singapore; U.S. National
Science Foundation [DEB 0743491]
FX We thank the Biodiversity Management Bureau (BMB), formerly the
Protected Areas and Wildlife Bureau (PAWB), of the Philippine Department
of Environment and Natural Resources (DENR) for facilitating collecting
and export permits necessary for this and related studies. In particular
we thank M. Lim, C. Custodio, J. L. De Leon, and A. Tagtag for their
assistance and support. We thank Cagayan and Isabela provincial DENR and
PENRO officers and staff for logistical support (Brown et al., 2013b).
Financial support for fieldwork was provided to ACD by a grant from the
Rufford Foundation and the National University of Singapore and to RMB
by a grant from the U.S. National Science Foundation (DEB 0743491). We
thank J. Fernandez and K. Hesed for field assistance and C. D. Siler for
assistance with the map in Figure 1. For the loans of specimens and
hospitality during research visits to collections, we thank C. McCarthy
(BMNH); J. McCoy, E. Censky, and S. Rogers (CM); J. Vindum, R. Drewes,
and A. Leviton (CAS); A. Resetar (FMNH); J. Rosado (MCZ); J. Barns
(PNM); K. Klemmer and G. Kohler (SMF); and D. Auth (UF). Critical
reviews of the manuscript were provided by two anonymous reviewers.
NR 40
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U1 0
U2 0
PU SOC STUDY AMPHIBIANS REPTILES
PI ST LOUIS
PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST
LOUIS, MO 63103 USA
SN 0022-1511
EI 1937-2418
J9 J HERPETOL
JI J. Herpetol.
PD MAR
PY 2016
VL 50
IS 1
BP 157
EP 168
DI 10.1670/14-104
PG 12
WC Zoology
SC Zoology
GA DF8OO
UT WOS:000371617900025
ER
PT J
AU Banton, SA
Soltowl, QA
Liu, KH
Uppal, K
Promislow, DEL
Power, ML
Tardif, SD
Wachtman, LM
Jones, DP
AF Banton, Sophia A.
Soltowl, Quinlyn A.
Liu, Ken H.
Uppal, Karan
Promislow, Daniel E. L.
Power, Michael L.
Tardif, Suzette D.
Wachtman, Lynn M.
Jones, Dean P.
TI Plasma Metabolomics of Common Marmosets (Callithrix jacchus) to Evaluate
Diet and Feeding Husbandry
SO JOURNAL OF THE AMERICAN ASSOCIATION FOR LABORATORY ANIMAL SCIENCE
LA English
DT Article
ID MONKEYS; AGE; MITOCHONDRIA; PERFORMANCE; BEHAVIORS; PROFILES; DISEASES;
PRIMATE; DECLINE; CARE
AB Common marmosets (Callithrix jacchus) are an important NHP model for the study of human aging and age-related diseases. However, the full potential of marmosets as a research model has not been realized due to a lack of evidence-based, standardized procedures for their captive management, especially regarding diet and feeding husbandry. In the present study, we conducted a high-resolution metabolomics analysis of plasma from marmosets from a 3-mo dietary crossover study to determine whether significant metabolic differences occur with a semisynthetic chemically defined (purified) diet as needed for controlled nutrition research. Marmosets were fed a standard, diverse-ingredient diet, followed by a semisynthetic purified diet, and then were switched back to the standard diet. The standard diet used in this analysis was specific to the animal facility, but it is similar in content to the diets currently used for other marmoset colonies. High-resolution metabolomics of plasma with liquid chromatography mass spectrometry and bioinformatics was used to measure metabolic differences. The concentration of the essential amino acids methionine, leucine/isoleucine, lysine, and threonine were higher when marmosets were fed the purified diet. In contrast, phenylalanine concentrations were higher during exposure to the standard diet. In addition, metabolic pathway enrichment and analysis revealed differences among metabolites associated with dopamine metabolism and the carnitine shuttle. These results show that diet-associated differences in metabolism occur in marmosets and suggest that additional nutritional studies with detailed physiologic characterization are needed to optimize standard and purified diets for common marmosets.
C1 [Banton, Sophia A.; Soltowl, Quinlyn A.; Liu, Ken H.; Uppal, Karan; Jones, Dean P.] Emory Univ, Dept Med, Clin Biomarkers Lab, Div Pulm Allergy & Crit Care Med, Atlanta, GA 30322 USA.
[Promislow, Daniel E. L.] Univ Washington, Dept Pathol, Seattle, WA 98195 USA.
[Power, Michael L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Nutr Lab, Washington, DC USA.
[Tardif, Suzette D.] Southwest Natl Primate Res Ctr, San Antonio, TX USA.
[Wachtman, Lynn M.] Harvard Univ, New England Primate Res Ctr, Southborough, MA USA.
[Soltowl, Quinlyn A.] Amplyx Pharmaceut, San Diego, CA USA.
[Wachtman, Lynn M.] MIT, Div Comparat Med, Cambridge, MA 02139 USA.
RP Jones, DP (reprint author), Emory Univ, Dept Med, Clin Biomarkers Lab, Div Pulm Allergy & Crit Care Med, Atlanta, GA 30322 USA.
EM dpjones@emory.edu
FU NIA [AG038746]; Southwest National Primate Research Center [P51
OD011133]; [RR02022]; [DK077639]
FX This research was supported by NIA grant AG038746 (DPJ, DEP, LW). The
development of the purified diet was supported by grants RR02022 (ST)
and DK077639 (ST and MP) and by the Southwest National Primate Research
Center (P51 OD011133).
NR 37
TC 0
Z9 0
U1 5
U2 6
PU AMER ASSOC LABORATORY ANIMAL SCIENCE
PI MEMPHIS
PA 9190 CRESTWYN HILLS DR, MEMPHIS, TN 38125 USA
SN 1559-6109
J9 J AM ASSOC LAB ANIM
JI J. Amer. Assoc. Lab. Anim. Sci.
PD MAR
PY 2016
VL 55
IS 2
BP 137
EP 146
PG 10
WC Veterinary Sciences; Zoology
SC Veterinary Sciences; Zoology
GA DG1SR
UT WOS:000371848300002
PM 27025803
ER
PT J
AU Galbany, J
Imanizabayo, O
Romero, A
Vecellio, V
Glowacka, H
Cranfield, MR
Bromage, TG
Mudakikwa, A
Stoinski, TS
McFarlin, SC
AF Galbany, Jordi
Imanizabayo, Olive
Romero, Alejandro
Vecellio, Veronica
Glowacka, Halszka
Cranfield, Michael R.
Bromage, Timothy G.
Mudakikwa, Antoine
Stoinski, Tara S.
McFarlin, Shannon C.
TI Tooth wear and feeding ecology in mountain gorillas from Volcanoes
National Park, Rwanda
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Article
DE dentine exposure; aging; diet; Gorilla beringei beringei
ID LEMURS LEMUR-CATTA; DENTAL WEAR; MOLAR WEAR; BEHAVIOR; AVAILABILITY;
INFORMATION; PHYTOLITHS; DYNAMICS; RESOURCE; BERINGEI
AB ObjectivesEcological factors have a dramatic effect on tooth wear in primates, although it remains unclear how individual age contributes to functional crown morphology. The aim of this study is to determine how age and individual diet are related to tooth wear in wild mountain gorillas (Gorilla beringei beringei) from Volcanoes National Park, Rwanda.
Material and MethodsWe calculated the percent of dentine exposure (PDE) for all permanent molars (M1-M3) of known-age mountain gorillas (N=23), to test whether PDE varied with age using regression analysis. For each molar position, we also performed stepwise multiple linear regression to test the effects of age and percentage of time spent feeding on different food categories on PDE, for individuals subject to long-term observational studies by the Dian Fossey Gorilla Fund International's Karisoke Research Center.
ResultsPDE increased significantly with age for both sexes in all molars. Moreover, a significant effect of gritty plant root consumption on PDE was found among individuals. Our results support prior reports indicating reduced tooth wear in mountain gorillas compared to western gorillas, and compared to other known-aged samples of primate taxa from forest and savanna habitats.
DiscussionOur findings corroborate that mountain gorillas present very low molar wear, and support the hypothesis that age and the consumption of particular food types, namely roots, are significant determinants of tooth wear variation in mountain gorillas. Future research should characterize the mineral composition of the soil in the Virunga habitat, to test the hypothesis that the physical and abrasive properties of gritty foods such as roots influence intra- and interspecific patterns of tooth wear. Am J Phys Anthropol 159:457-465, 2016. (c) 2015 Wiley Periodicals, Inc.
C1 [Galbany, Jordi; McFarlin, Shannon C.] George Washington Univ, Dept Anthropol, Ctr Adv Study Human Paleobiol, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA.
[Imanizabayo, Olive; Vecellio, Veronica; Stoinski, Tara S.] Dian Fossey Gorilla Fund Int, Atlanta, GA USA.
[Romero, Alejandro] Univ Alicante, Dept Biotechnol, E-03080 Alicante, Spain.
[Glowacka, Halszka] Arizona State Univ, Inst Human Origins, Tempe, AZ USA.
[Cranfield, Michael R.] Univ Calif Davis, Mt Gorilla Vet Project, Davis, CA 95616 USA.
[Bromage, Timothy G.] NYU, Coll Dent, Hard Tissue Res Unit, New York, NY 10003 USA.
[Mudakikwa, Antoine] Dept Tourism & Conservat, Rwanda Dev Board, Kigali, Rwanda.
[McFarlin, Shannon C.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA.
RP Galbany, J (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Human Paleobiol, 800 22nd St NW,Ste 6000, Washington, DC 20052 USA.
EM jgalbany@gwu.edu
RI Romero, Alejandro/J-9405-2014;
OI Romero, Alejandro/0000-0002-5743-0613; Galbany,
Jordi/0000-0001-6724-3451
FU National Science Foundation [BCS 0852866, 0964944]; Leakey Foundation;
National Geographic Society's Committee for Exploration and Research;
Center and Institute Facilitating Fund of George Washington University;
German Federal Ministry of Education and Research; Alexander von
Humboldt Foundation
FX Grant sponsor: National Science Foundation; Grant numbers: BCS 0852866,
0964944; Grant sponsors: The Leakey Foundation; National Geographic
Society's Committee for Exploration and Research; the Center and
Institute Facilitating Fund of The George Washington University; the
2010 Max Planck Research Award endowed by the German Federal Ministry of
Education and Research to the Max Planck Society; Alexander von Humboldt
Foundation.
NR 44
TC 2
Z9 2
U1 11
U2 24
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD MAR
PY 2016
VL 159
IS 3
BP 457
EP 465
DI 10.1002/ajpa.22897
PG 9
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA DF1KD
UT WOS:000371097400008
PM 26597436
ER
PT J
AU Kirk, B
Conroy, K
Prsa, A
Abdul-Masih, M
Kochoska, A
Matijevic, G
Hambleton, K
Barclay, T
Bloemen, S
Boyajian, T
Doyle, LR
Fulton, BJ
Hoekstra, AJ
Jek, K
Kane, SR
Kostov, V
Latham, D
Mazeh, T
Orosz, JA
Pepper, J
Quarles, B
Ragozzine, D
Shporer, A
Southworth, J
Stassun, K
Thompson, SE
Welsh, WF
Agol, E
Derekas, A
Devor, J
Fischer, D
Green, G
Gropp, J
Jacobs, T
Johnston, C
LaCourse, DM
Saetre, K
Schwengeler, H
Toczyski, J
Werner, G
Garrett, M
Gore, J
Martinez, AO
Spitzer, I
Stevick, J
Thomadis, PC
Vrijmoet, EH
Yenawine, M
Batalha, N
Borucki, W
AF Kirk, Brian
Conroy, Kyle
Prsa, Andrej
Abdul-Masih, Michael
Kochoska, Angela
Matijevic, Gal
Hambleton, Kelly
Barclay, Thomas
Bloemen, Steven
Boyajian, Tabetha
Doyle, Laurance R.
Fulton, B. J.
Hoekstra, Abe Johannes
Jek, Kian
Kane, Stephen R.
Kostov, Veselin
Latham, David
Mazeh, Tsevi
Orosz, Jerome A.
Pepper, Joshua
Quarles, Billy
Ragozzine, Darin
Shporer, Avi
Southworth, John
Stassun, Keivan
Thompson, Susan E.
Welsh, William F.
Agol, Eric
Derekas, Aliz
Devor, Jonathan
Fischer, Debra
Green, Gregory
Gropp, Jeff
Jacobs, Tom
Johnston, Cole
LaCourse, Daryll Matthew
Saetre, Kristian
Schwengeler, Hans
Toczyski, Jacek
Werner, Griffin
Garrett, Matthew
Gore, Joanna
Martinez, Arturo O.
Spitzer, Isaac
Stevick, Justin
Thomadis, Pantelis C.
Vrijmoet, Eliot Halley
Yenawine, Mitchell
Batalha, Natalie
Borucki, William
TI KEPLER ECLIPSING BINARY STARS. VII. THE CATALOG OF ECLIPSING BINARIES
FOUND IN THE ENTIRE KEPLER DATA SET
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; catalogs; methods: data analysis; methods:
numerical; stars: fundamental parameters; stars: statistics
ID SMALL-MAGELLANIC-CLOUD; TRANSITING CIRCUMBINARY PLANET; APSIDAL-MOTION
TEST; STELLAR EVOLUTION; CLOSE BINARIES; PHOTOMETRIC SOLUTIONS; DISTANCE
INDICATORS; DATA RELEASE; CM DRACONIS; SPACED DATA
AB The primary Kepler Mission provided nearly continuous monitoring of similar to 200,000 objects with unprecedented photometric precision. We present the final catalog of eclipsing binary systems within the 105 deg(2) Kepler field of view. This release incorporates the full extent of the data from the primary mission (Q0-Q17 Data Release). As a result, new systems have been added, additional false positives have been removed, ephemerides and principal parameters have been recomputed, classifications have been revised to rely on analytical models, and eclipse timing variations have been computed for each system. We identify several classes of systems including those that exhibit tertiary eclipse events, systems that show clear evidence of additional bodies, heartbeat systems, systems with changing eclipse depths, and systems exhibiting only one eclipse event over the duration of the mission. We have updated the period and galactic latitude distribution diagrams and included a catalog completeness evaluation. The total number of identified eclipsing and ellipsoidal binary systems in the Kepler field of view has increased to 2878, 1.3% of all observed Kepler targets. An online version of this catalog with downloadable content and visualization tools is maintained at http://keplerEBs.villanova.edu.
C1 [Kirk, Brian] North Amer ALMA Sci Ctr, Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Kirk, Brian; Conroy, Kyle; Gropp, Jeff; Johnston, Cole; Werner, Griffin] Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster Ave, Villanova, PA 19085 USA.
[Conroy, Kyle; Prsa, Andrej; Abdul-Masih, Michael; Matijevic, Gal] Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA.
[Abdul-Masih, Michael] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, 110 8th St, Troy, NY 12180 USA.
[Kochoska, Angela] Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia.
[Hambleton, Kelly] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Barclay, Thomas] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94035 USA.
[Bloemen, Steven] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Boyajian, Tabetha] Yale Univ, JW Gibbs Lab, 260 Whitney Ave, New Haven, CT 06511 USA.
[Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA.
[Doyle, Laurance R.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Fulton, B. J.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Kane, Stephen R.] San Francisco State Univ, 1600 Holloway Ave, San Francisco, CA 94132 USA.
[Kostov, Veselin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Latham, David] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Mazeh, Tsevi] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel.
[Orosz, Jerome A.; Welsh, William F.; Garrett, Matthew; Gore, Joanna; Martinez, Arturo O.; Spitzer, Isaac; Stevick, Justin; Thomadis, Pantelis C.; Vrijmoet, Eliot Halley; Yenawine, Mitchell] San Diego State Univ, 5500 Campanile Dr, San Diego, CA 92182 USA.
[Pepper, Joshua] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA.
[Quarles, Billy] NASA, Ames Res Ctr, Astrobiol & Space Sci Div MS 245 3, Moffett Field, CA 94035 USA.
[Ragozzine, Darin] Florida Inst Technol, Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Southworth, John] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Stassun, Keivan] Vanderbilt Univ, Nashville, TN 37240 USA.
[Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Derekas, Aliz] ELTE Gothard Astrophys Observ, Szent Imre Herceg U 112, H-9704 Szombathely, Hungary.
[Derekas, Aliz] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Debrecen, Hungary.
[Devor, Jonathan] Tel Aviv Univ, Dept Astrophys, IL-69978 Tel Aviv, Israel.
[Fischer, Debra] Yale Univ, New Haven, CT 06520 USA.
[Green, Gregory] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA.
[Schwengeler, Hans] Univ Basel, Astron Inst, Venusstr 7, CH-4102 Binningen, Switzerland.
[Toczyski, Jacek] Univ Virginia, 4040 Lewis & Clark Dr, Charlottesville, VA 22911 USA.
[Batalha, Natalie] San Jose State Univ, One Washington Sq, San Jose, CA 95192 USA.
[Borucki, William] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kirk, B (reprint author), North Amer ALMA Sci Ctr, Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.; Kirk, B (reprint author), Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster Ave, Villanova, PA 19085 USA.
EM bkirk@nrao.edu; kyle.conroy@vanderbilt.edu; aprsa@villanova.edu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; /0000-0002-0802-9145; Pepper,
Joshua/0000-0002-3827-8417
FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASAs
Science Mission Directorate; NOAO survey program [11A-0022]; NASA/SETI
[08-SC-1041]; NSF RUI [AST-05-07542]; Postdoctoral Fellowship Programme
of the Hungarian Academy of Sciences; Janos Bolyai Research Scholarship
of the Hungarian Academy of Sciences; Lendulet Young Researchers
Programme of the Hungarian Academy of Sciences; European Communitys
Seventh Framework Programme (FP7) [269194 (IRSES/ASK), 312844];
Hungarian National Research, Development and Innovation Office-NKFIH
[K-1157709]; [ADAP14-0245]; [ADAP12-0172]
FX All of the data presented in this paper were obtained from the
Multimission Archive at the Space Telescope Science Institute (MAST).
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-Hubble Space Telescope data is provided by the NASA Office of Space
Science via grant NNX09AF08G and by other grants and contracts. Funding
for this Discovery Mission is provided by NASAs Science Mission
Directorate. Spectroscopic follow-up data are made available through
NOAO survey program 11A-0022. This work is funded in part by the
NASA/SETI subcontract 08-SC-1041 and NSF RUI AST-05-07542. B.Q. was
supported by an appointment to the NASA Postdoctoral Program at the Ames
Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA. T.S.B. acknowledges support from
ADAP14-0245 and ADAP12-0172. A.D. has been supported by the Postdoctoral
Fellowship Programme of the Hungarian Academy of Sciences, the Janos
Bolyai Research Scholarship of the Hungarian Academy of Sciences,
Lendulet-2009 Young Researchers Programme of the Hungarian Academy of
Sciences, the European Communitys Seventh Framework Programme
(FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK) and no.
312844 (SPACEINN). A. D. has also been supported by the Hungarian
National Research, Development and Innovation Office-NKFIH K-1157709.
NR 81
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Z9 17
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2016
VL 151
IS 3
AR 68
DI 10.3847/0004-6256/151/3/68
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF3MT
UT WOS:000371249100020
ER
PT J
AU Soley-Guardia, M
Gutierrez, EE
Thomas, DM
Ochoa, J
Aguilera, M
Anderson, RP
AF Soley-Guardia, Mariano
Gutierrez, Eliecer E.
Thomas, Darla M.
Ochoa-G, Jose
Aguilera, Marisol
Anderson, Robert P.
TI Are we overestimating the niche? Removing marginal localities helps
ecological niche models detect environmental barriers
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Gallery forests; habitat connectivity; niche conservatism; Paraguana;
small mammals; soft allopatry
ID SPECIES GEOGRAPHIC DISTRIBUTIONS; CONSERVATION BIOLOGY; SPECIATION;
VENEZUELA; EVOLUTION; MAXENT; BIAS; PERFORMANCE; ADAPTATION; AMERICA
AB Correlative ecological niche models (ENMs) estimate species niches using occurrence records and environmental data. These tools are valuable to the field of biogeography, where they are commonly used to infer potential connectivity among populations. However, a recent study showed that when locally relevant environmental data are not available, records from patches of suitable habitat protruding into otherwise unsuitable regions (e.g., gallery forests within dry areas) can lead to overestimations of species niches and their potential distributions. Here, we test whether this issue obfuscates detection of an obvious environmental barrier existing in northern Venezuela - that of the hot and xeric lowlands separating the Peninsula de Paraguana from mainland South America. These conditions most likely promote isolation between mainland and peninsular populations of three rodent lineages occurring in mesic habitat in this region. For each lineage, we calibrated optimally parameterized ENMs using mainland records only, and leveraged existing habitat descriptions to assess whether those assigned low suitability values corresponded to instances where the species was collected within locally mesic conditions amidst otherwise hot dry areas. When this was the case, we built an additional model excluding these records. We projected both models onto the peninsula and assessed whether they differed in their ability to detect the environmental barrier. For the two lineages in which we detected such problematic records, only the models built excluding them detected the barrier, while providing additional insights regarding peninsular populations. Overall, the study reveals how a simple procedure like the one applied here can deal with records problematic for ENMs, leading to better predictions regarding the potential effects of the environment on lineage divergence.
C1 [Soley-Guardia, Mariano; Gutierrez, Eliecer E.; Thomas, Darla M.; Anderson, Robert P.] CUNY City Coll, Dept Biol, 138Th St & Convent Ave, New York, NY 10031 USA.
[Soley-Guardia, Mariano; Gutierrez, Eliecer E.; Anderson, Robert P.] CUNY, Grad Ctr, New York, NY 10021 USA.
[Gutierrez, Eliecer E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Ochoa-G, Jose] Cabanas Bougainvillae, Los Taques, Venezuela.
[Aguilera, Marisol] Univ Simon Bolivar, Dept Estudios Ambient, Caracas, Venezuela.
[Anderson, Robert P.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA.
RP Soley-Guardia, M (reprint author), CUNY City Coll, Dept Biol, 138Th St & Convent Ave, New York, NY 10031 USA.
EM msoley@sci.ccny.cuny.edu
RI Gutierrez, Eliecer/D-5703-2014
OI Gutierrez, Eliecer/0000-0001-6790-8185
FU U.S. National Science Foundation [DEB-0717357, DEB-1119915]; Graduate
Center of City University of New York; City College (Academy for
Professional Preparation); Luis Stokes Alliance for Minority
Participation; Smithsonian Institution (Division of Mammals);
Smithsonian Institution (Buck Postdoctoral Fellowship)
FX U.S. National Science Foundation ('DEB-0717357', 'DEB-1119915');
Graduate Center of the City University of New York; City College
(Academy for Professional Preparation); Luis Stokes Alliance for
Minority Participation; Smithsonian Institution (Buck Postdoctoral
Fellowship; Division of Mammals).
NR 71
TC 2
Z9 2
U1 8
U2 28
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD MAR
PY 2016
VL 6
IS 5
BP 1267
EP 1279
DI 10.1002/ece3.1900
PG 13
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DF3CP
UT WOS:000371221600001
PM 26848385
ER
PT J
AU Cramer, ERA
Stensrud, E
Marthinsen, G
Hogner, S
Johannessen, LE
Laskemoen, T
Eybert, MC
Slagsvold, T
Lifjeld, JT
Johnsen, A
AF Cramer, Emily R. A.
Stensrud, Even
Marthinsen, Gunnhild
Hogner, Silje
Johannessen, Lars Erik
Laskemoen, Terje
Eybert, Marie-Christine
Slagsvold, Tore
Lifjeld, Jan T.
Johnsen, Arild
TI Sperm performance in conspecific and heterospecific female fluid
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Cryptic female choice; postcopulatory prezygotic barriers; sexual
selection; speciation; sperm competition; sperm motility; sperm velocity
ID POSTCOPULATORY SEXUAL SELECTION; PASSERINE BIRDS; REPRODUCTIVE
ISOLATION; FERTILIZATION SUCCESS; HIRUNDO-RUSTICA; IN-VITRO; EVOLUTION;
SPECIATION; SPERMATOZOA; COMPETITION
AB Divergent sexual selection within allopatric populations may result in divergent sexual phenotypes, which can act as reproductive barriers between populations upon secondary contact. This hypothesis has been most tested on traits involved in precopulatory sexual selection, with less work focusing on traits that act after copulation and before fertilization (i.e., postcopulatory prezygotic traits), particularly in internally fertilizing vertebrates. However, postcopulatory sexual selection within species can also drive trait divergence, resulting in reduced performance of heterospecific sperm within the female reproductive tract. Such incompatibilities, arising as a by-product of divergent postcopulatory sexual selection in allopatry, can represent reproductive barriers, analogous to species-assortative mating preferences. Here, we tested for postcopulatory prezygotic reproductive barriers between three pairs of taxa with diverged sperm phenotypes and moderate-to-high opportunity for postcopulatory sexual selection (barn swallows Hirundo rustica versus sand martins Riparia riparia, two subspecies of bluethroats, Luscinia svecica svecica versus L. s. namnetum, and great tits Parus major versus blue tits Cyanistes caeruleus). We tested sperm swimming performance in fluid from the outer reproductive tract of females, because the greatest reduction in sperm number in birds occurs as sperm swim across the vagina. Contrary to our expectations, sperm swam equally well in fluid from conspecific and heterospecific females, suggesting that postcopulatory prezygotic barriers do not act between these taxon pairs, at this stage between copulation and fertilization. We therefore suggest that divergence in sperm phenotypes in allopatry is insufficient to cause widespread postcopulatory prezygotic barriers in the form of impaired sperm swimming performance in passerine birds.
C1 [Cramer, Emily R. A.; Stensrud, Even; Marthinsen, Gunnhild; Hogner, Silje; Johannessen, Lars Erik; Laskemoen, Terje; Lifjeld, Jan T.; Johnsen, Arild] Univ Oslo, Nat Hist Museum, POB 1172, N-0318 Oslo, Norway.
[Eybert, Marie-Christine] Univ Rennes 1, EA7316, 263 Ave Gen Leclerc, F-35042 Rennes, France.
[Slagsvold, Tore] Univ Oslo, Ctr Ecol & Evolutionary Synth, Dept Biosci, POB 1066, N-0316 Oslo, Norway.
RP Cramer, ERA (reprint author), Smithsonian Conservat Biol Inst, POB 37012 MRC5503, Washington, DC 20008 USA.; Cramer, ERA (reprint author), Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA.
EM erc25@cornell.edu
RI Lifjeld, Jan/B-1978-2008
OI Lifjeld, Jan/0000-0002-9172-9985
FU Norges Forskningsrad [213592]
FX Norges Forskningsrad (Grant/Award Number: '213592')
NR 80
TC 1
Z9 2
U1 7
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD MAR
PY 2016
VL 6
IS 5
BP 1363
EP 1377
DI 10.1002/ece3.1977
PG 15
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DF3CP
UT WOS:000371221600009
PM 26855769
ER
PT J
AU Geddes, JA
Martin, RV
Boys, BL
van Donkelaar, A
AF Geddes, Jeffrey A.
Martin, Randall V.
Boys, Brian L.
van Donkelaar, Aaron
TI Long-Term Trends Worldwide in Ambient NO2 Concentrations Inferred from
Satellite Observations
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
ID FINE PARTICULATE MATTER; NITROGEN-DIOXIDE; AIR-POLLUTION; UNITED-STATES;
TIME-SERIES; ECONOMIC RECESSION; TROPOSPHERIC NO2; MORTALITY; EMISSIONS;
HEALTH
AB BACKGROUND: Air pollution is associated with morbidity and premature mortality. Satellite remote sensing provides globally consistent decadal-scale observations of ambient nitrogen dioxide (NO2) pollution.
OBJECTIVE: We determined global population-weighted annual mean NO2 concentrations from 1996 through 2012.
METHODS: We used observations of NO2 tropospheric column densities from three satellite instruments in combination with chemical transport modeling to produce a global 17-year record of ground-level NO2 at 0.1 degrees x 0.1 degrees resolution. We calculated linear trends in population-weighted annual mean NO2 (PWMNO2) concentrations in different regions around the world.
RESULTS: We found that PWMNO2 in high-income North America (Canada and the United States) decreased more steeply than in any other region, having declined at a rate of -4.7%/ year [95% confidence interval (CI): -5.3, -4.1]. PWMNO2 decreased in western Europe at a rate of -2.5%/year (95% CI: -3.0, -2.1). The highest PWMNO2 occurred in high-income Asia Pacific (predominantly Japan and South Korea) in 1996, with a subsequent decrease of -2.1%/ year (95% CI: -2.7, -1.5). In contrast, PWMNO2 almost tripled in East Asia (China, North Korea, and Taiwan) at a rate of 6.7%/ year (95% CI: 6.0, 7.3). The satellite-derived estimates of trends in ground-level NO2 were consistent with regional trends inferred from data obtained from ground-station monitoring networks in North America (within 0.7%/ year) and Europe (within 0.3%/year). Our rankings of regional average NO2 and long-term trends differed from the satellite-derived estimates of fine particulate matter reported elsewhere, demonstrating the utility of both indicators to describe changing pollutant mixtures.
CONCLUSIONS: Long-term trends in satellite-derived ambient NO2 provide new information about changing global exposure to ambient air pollution. Our estimates are publicly available at http://fizz.phys.dal.ca/similar to atmos/martin/?page_id=232.
C1 [Geddes, Jeffrey A.; Martin, Randall V.; Boys, Brian L.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Box 15000, Halifax, NS B3H 4R2, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Geddes, JA (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Box 15000, Halifax, NS B3H 4R2, Canada.
EM jeff.geddes@dal.ca
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU Natural Science and Engineering Research Council (NSERC) of Canada;
NSERC CREATE IACPES (Collaborative Research and Training Experience
Program: Integrating Atmospheric Chemistry and Physics from Earth to
Space); Health Canada
FX This work was supported by the Natural Science and Engineering Research
Council (NSERC) of Canada and by Health Canada. Funding for J.A.G. was
supported by NSERC CREATE IACPES (Collaborative Research and Training
Experience Program: Integrating Atmospheric Chemistry and Physics from
Earth to Space; http://iacpes.info.yorku.ca/).
NR 46
TC 7
Z9 8
U1 9
U2 29
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
EI 1552-9924
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD MAR
PY 2016
VL 124
IS 3
BP 281
EP 289
DI 10.1289/ehp.1409567
PG 9
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA DF6CJ
UT WOS:000371442500013
PM 26241114
ER
PT J
AU van Soest, R
Rutzler, K
Sim, CJ
AF van Soest, Rob
Ruetzler, Klaus
Sim, Chung-Ja
TI Crooked Anthos: proposed subgeneric status of Jia (Porifera,
Poecilosclerida), with descriptions of four new species
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE sponges; new species; Antho; Jia; Galapagos; Red Sea; Indonesia; Korea
ID WATERS
AB Jia De Laubenfels, 1930 was erected to accommodate Californian Jia jia, a microcionid sponge possessing a unique J-shaped microsclere, subsequently named croca (crook, shepherd's staff). In later revisions, the genus was assigned to the synonymy of Antho Gray, 1867 because of similarity in skeletal and spicular characters with that large worldwide genus. Over the years, two additional species, one Atlantic, one from the Tropical East Pacific, were found to possess the crocae, and here four additional species with these intriguing spicules are described from Indo-West and East Pacific localities. It appears that now seven species, all Antho-like, are known to possess crocae, together distributed over all three oceans. This leads us to hypothesize that crocae are a shared character of a monophyletic group of Antho species and accordingly we propose to revive Jia as a subgenus of Antho. The four new species are Antho (Jia) galapagosensis sp. nov., Antho (Jia) lithisticola sp. nov., Antho (Jia) wunschorum sp. nov. and Antho (Jia) ramosa sp. nov.
C1 [van Soest, Rob] Nat Biodivers Ctr, POB 9517, NL-2300 RA Leiden, Netherlands.
[Ruetzler, Klaus] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Sim, Chung-Ja] Hannam Univ, Dept Biol Sci & Biotechnol, Daejeon 305811, South Korea.
RP van Soest, R (reprint author), Nat Biodivers Ctr, POB 9517, NL-2300 RA Leiden, Netherlands.
EM rob.vansoest@naturalis.nl
NR 29
TC 0
Z9 0
U1 4
U2 6
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD MAR
PY 2016
VL 96
IS 2
SI SI
BP 221
EP 235
DI 10.1017/S002531541400191X
PG 15
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DF2HR
UT WOS:000371163700002
ER
PT J
AU Freeman, CJ
Easson, CG
Baker, DM
AF Freeman, Christopher J.
Easson, Cole G.
Baker, David M.
TI Niche structure of marine sponges from temperate hard-bottom habitats
within Gray's Reef National Marine Sanctuary
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Gray's Reef; latitudinal gradient; isotopic niche space; microbes;
microbial abundance; Porifera; standard ellipse area; stable isotopes;
symbiosis; temperate
ID STABLE-ISOTOPE RATIOS; MICROBIAL COMMUNITIES; CYANOBACTERIAL SYMBIONTS;
ANTARCTIC SPONGES; MISKITO CAYS; FLORIDA-KEYS; CORAL; DIVERSITY;
ECOLOGY; ABUNDANCE
AB Many species of marine sponges on tropical reefs host abundant and diverse symbiont communities capable of varied metabolic pathways. While such communities may confer a nutritional benefit to some hosts (termed High Microbial Abundance (HMA) sponges), other sympatric species host only sparse symbiont communities (termed Low Microbial Abundance (LMA) sponges) and obtain a majority of their C and N from local sources. Sponge communities are widespread across large latitudinal gradients, however, and recent evidence suggests that these symbioses may also extend beyond the tropics. We investigated the role that symbionts play in the ecology of sponges from the temperate, hard-bottom reefs of Gray's Reef National Marine Sanctuary by calculating the niche size (as standard ellipse area (SEA(c))) and assessing the relative placement of five HMA and four LMA sponge species within bivariate (delta C-13 and delta N-15) isotopic space. Although photosymbiont abundance was low across most of these species, sponges were widespread across isotopic niche space, implying that microbial metabolism confers an ecological benefit to temperate sponges by expanding host metabolic capability. To examine how these associations vary across a latitudinal gradient, we also compared the relative placement of temperate and tropical conspecifics within isotopic space. Surprisingly, shifts in sponge delta C-13 and delta N-15 values between these regions suggest a reduced reliance on symbiontderived nutrients in temperate sponges compared with their tropical conspecifics. Despite this, symbiotic sponges in temperate systems likely have a competitive advantage, allowing them to grow and compete for space within these habitats.
C1 [Freeman, Christopher J.] Smithsonian Marine Stn, Ft Pierce, FL USA.
[Easson, Cole G.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA.
[Baker, David M.] Univ Hong Kong, Sch Biol Sci, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China.
[Baker, David M.] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China.
RP Freeman, CJ (reprint author), Smithsonian Marine Stn, Ft Pierce, FL USA.
EM freemanc@si.edu
FU Marine Global Earth Observatory (MarineGEO) project at the Smithsonian
Institution
FX Financial support for this project was provided to CJF as part of a
postdoctoral fellowship with the Marine Global Earth Observatory
(MarineGEO) project at the Smithsonian Institution.
NR 46
TC 0
Z9 0
U1 4
U2 14
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD MAR
PY 2016
VL 96
IS 2
SI SI
BP 559
EP 565
DI 10.1017/S0025315415000363
PG 7
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DF2HR
UT WOS:000371163700030
ER
PT J
AU Straker, LC
AF Straker, Lorian Cobra
TI Quantitative characterization and comparative study of feather
melanosome internal morphology using surface analysis
SO MICRON
LA English
DT Article
DE Transmission Electron Microscopy; Surface analysis; Morphology;
Melanosome; Storm petrel; Feather development
ID IN-VITRO; MELANIN; MELANOCYTES; EVOLUTION; MORPHOGENESIS; REGENERATION;
ELONGATION; ASYMMETRY; SWALLOWS; MODEL
AB A successful feather development implies in a precise orchestration of cells in the follicle, which culminates in one of the most complex epidermal structures in nature. Melanocytes contribute to the final structure by delivering melanosomes to the barb and barbule cells. Disturbance to the tissue during the feather growth can damage the final structure. Here, melanosomes seen in an unusual outgrowth on the barb cortex of a flight feather are reported and compared to commonly observed melanosomes embedded in the cortex. Transmission Electron Microscopy in scanning-transmission mode (STEM) generated images coupled with secondary electron detection. The two classes of melanosomes were registered on images combining transmitted and secondary electron signals. Image processing allowed surface analyses of roughness and texture of the internal morphology of these organelles. Results showed that the two classes of melanosomes are significantly distinct internally, indicating that different physiological processes up to feather maturation could have occurred. Surface analysis methods are not regularly used in cell biology studies, but here it is shown that it has great potential for microscopic image analysis, which could add robust information to studies of cell biology events. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Straker, Lorian Cobra] Natl Museum Nat Hist, Smithsonian Inst, Div Birds, E-600,MRC 116,10th & Constitut Ave NW, Washington, DC 20560 USA.
[Straker, Lorian Cobra] Univ Fed Rio de Janeiro, Inst Biofis Carlos Chagas Filho, Lab Ultraestrutura Celular Hertha Meyer, Ilha Fundao, BR-21949900 Rio De Janeiro, RJ, Brazil.
RP Straker, LC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Birds, E-600,MRC 116,10th & Constitut Ave NW, Washington, DC 20560 USA.; Straker, LC (reprint author), Univ Fed Rio de Janeiro, Inst Biofis Carlos Chagas Filho, Lab Ultraestrutura Celular Hertha Meyer, Ilha Fundao, BR-21949900 Rio De Janeiro, RJ, Brazil.
EM StrakerL@si.edu
RI Straker, Lorian/J-5560-2016
FU CAPES/Fulbright [BEX 0543/11-0]; CNPq [246819/2013-8]
FX The author thank Shawkey's Lab staff at Akron University, OH, and
especially Dr. Rafael Maia for his help during the work with the STEM
microscope; Dr. Marcos Raposo for specimen sampling from the
Ornithological Collection of the Museu Nacional/UFRJ; Marcia Attias,
Rachel Rachid and Daniel Goncalves for their help with samples
preparation and observation at IBCCF, UFRJ; Carla Dove (Smithsonian
Institution) for revising the first manuscript; and CAPES/Fulbright (BEX
0543/11-0) and CNPq (246819/2013-8) for financial support on scholarship
funding.
NR 32
TC 0
Z9 0
U1 1
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0968-4328
J9 MICRON
JI Micron
PD MAR
PY 2016
VL 82
BP 17
EP 24
DI 10.1016/j.micron.2015.12.007
PG 8
WC Microscopy
SC Microscopy
GA DF5CJ
UT WOS:000371369100003
PM 26760226
ER
PT J
AU Davis, AM
Unmack, PJ
Vari, RP
Betancur, R
AF Davis, Aaron M.
Unmack, Peter J.
Vari, Richard P.
Betancur-R, Ricardo
TI Herbivory Promotes Dental Disparification and Macroevolutionary Dynamics
in Grunters (Teleostei: Terapontidae), a Freshwater Adaptive Radiation
SO AMERICAN NATURALIST
LA English
DT Article
DE phenotypic disparification; herbivory; dentition; carnivory; trophic
shifts
ID R PACKAGE; STABILIZING SELECTION; PHYLOGENETIC ANALYSES; PRINCIPAL
COMPONENTS; EVOLUTIONARY RATES; CICHLID FISHES; DIVERSIFICATION; MARINE;
MORPHOLOGY; PATTERNS
AB Trophic shifts into new adaptive zones have played major (although often conflicting) roles in reshaping the evolutionary trajectories of many lineages. We analyze data on diet, tooth, and oral morphology and relate these traits to phenotypic disparification and lineage diversification rates across the ecologically diverse Terapontidae, a family of Australasian fishes. In contrast to carnivores and most omnivores, which have retained relatively simple, ancestral caniniform tooth shapes, herbivorous terapontids appear to have evolved a variety of novel tooth shapes at significantly faster rates to meet the demands of plant-based diets. The evolution of herbivory prompted major disparification, significantly expanding the terapontid adaptive phenotypic continuum into an entirely novel functional morphospace. There was minimal support for our hypothesis of faster overall rates of integrated tooth shape, spacing, and jaw biomechanical evolution in herbivorous terapontids in their entirety, compared with other trophic strategies. There was, however, considerable support for accelerated disparification within a diverse freshwater clade containing a range of specialized freshwater herbivores. While the evolutionary transition to herbivorous diets has played a central role in terapontid phenotypic diversification by pushing herbivores toward novel fitness peaks, there was little support for herbivory driving significantly higher lineage diversification compared with background rates across the family.
C1 [Davis, Aaron M.] James Cook Univ, Ctr Trop Water & Aquat Ecosyst Res TropWATER, Townsville, Qld 4811, Australia.
[Davis, Aaron M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
[Unmack, Peter J.] Univ Canberra, Inst Appl Ecol & Collaborat Res Network Murray Da, Canberra, ACT 2601, Australia.
[Vari, Richard P.; Betancur-R, Ricardo] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 159, Washington, DC 20013 USA.
[Betancur-R, Ricardo] Univ Puerto Rico Rio Piedras, Dept Biol, POB 23360, San Juan, PR 00931 USA.
RP Davis, AM (reprint author), James Cook Univ, Ctr Trop Water & Aquat Ecosyst Res TropWATER, Townsville, Qld 4811, Australia.; Davis, AM (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
EM aaron.davis@jcu.edu.au
FU Queensland Government Smithsonian Fellowship; Smithsonian P. Buck
Fellowship; National Science Foundation [DEB-1457184, DEB-1541491]
FX This study is dedicated to our friend and valued colleague Richard Vari
(recently deceased), whose early research provided the inspiration for
this article. We thank two anonymous reviewers and editorial reviews for
comments that greatly improved the manuscript. Research was funded in
part from a Queensland Government Smithsonian Fellowship to A.M.D., the
Smithsonian P. Buck Fellowship to R.B.-R., and National Science
Foundation awards DEB-1457184 and DEB-1541491 to R.B.-R. The Australian
Museum and the Smithsonian Natural History Museum are thanked for
specimen donation. K. Blake (James Cook University) and S. Whittaker
(Smithsonian National Museum of Natural History) are thanked for
scanning electron microscope assistance.
NR 79
TC 0
Z9 0
U1 7
U2 16
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0003-0147
EI 1537-5323
J9 AM NAT
JI Am. Nat.
PD MAR
PY 2016
VL 187
IS 3
BP 320
EP 333
DI 10.1086/684747
PG 14
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DE9KJ
UT WOS:000370955700006
PM 26913945
ER
PT J
AU Nomura, H
Tsukagoshi, T
Kawabe, R
Ishimoto, D
Okuzumi, S
Muto, T
Kanagawa, KD
Ida, S
Walsh, C
Millar, TJ
Bai, XN
AF Nomura, Hideko
Tsukagoshi, Takashi
Kawabe, Ryohei
Ishimoto, Daiki
Okuzumi, Satoshi
Muto, Takayuki
Kanagawa, Kazuhiro D.
Ida, Shigeru
Walsh, Catherine
Millar, T. J.
Bai, Xue-Ning
TI ALMA OBSERVATIONS OF A GAP AND A RING IN THE PROTOPLANETARY DISK AROUND
TW HYA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE molecular processes; planet-disk interactions; protoplanetary disks;
stars: individual (TW Hya); submillimeter: planetary systems
ID SUN-LIKE STAR; CO SNOW LINE; ORBITAL EVOLUTION; PLANET; REGION;
CHEMISTRY; DISCOVERY; NEBULA; HYDRAE; MASSES
AB We report the first detection of a gap and a ring in 336 GHz dust continuum emission from the protoplanetary disk around TW Hya, using the Atacama Large Millimeter/Submillimeter Array (ALMA). The gap and ring are located at around 25 and 41 au from the central star, respectively, and are associated with the CO snow line at similar to 30 au. The gap has a radial width of less than 15 au and a mass deficit of more than 23%, taking into account that the observations are limited to an angular resolution of similar to 15 au. In addition, the (CO)-C-13 and (CO)-O-18 J = 3 - 2 lines show a decrement in CO line emission throughout the disk, down to similar to 10 au, indicating a freeze-out of gas-phase CO onto grain surfaces and possible subsequent surface reactions to form larger molecules. The observed gap could be caused by gravitational interaction between the disk gas and a planet with a mass less than super-Neptune (2M(Neptune)), or could be the result of the destruction of large dust aggregates due to the sintering of CO ice.
C1 [Nomura, Hideko; Ishimoto, Daiki; Okuzumi, Satoshi] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Tsukagoshi, Takashi] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kawabe, Ryohei] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Kawabe, Ryohei] SOKENDAI Grad Univ Adv Studies, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Kawabe, Ryohei] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Ishimoto, Daiki] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, 1-24-2 Nishi Shinjuku, Tokyo 1638677, Japan.
[Kanagawa, Kazuhiro D.] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 0600819, Japan.
[Kanagawa, Kazuhiro D.] Univ Szczecin, Fac Math & Phys, Inst Phys, Wielkopolska 15, PL-70451 Szczecin, Poland.
[Kanagawa, Kazuhiro D.] Univ Szczecin, Fac Math & Phys, CASA, Wielkopolska 15, PL-70451 Szczecin, Poland.
[Ida, Shigeru] Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528550, Japan.
[Walsh, Catherine] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
[Nomura, Hideko; Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
RP Nomura, H (reprint author), Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.; Nomura, H (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM nomura@geo.titech.ac.jp
OI Kanagawa, Kazuhiro/0000-0001-7235-2417; Millar, Tom/0000-0001-5178-3656
FU JSPS KAKENHI [23103004]; Netherlands Organisation for Scientific
Research [639.041.335]; STFC; [23103005]; [25108004]; [25400229];
[15H03646]
FX We would like to thank the referee for comments that improved our paper.
We are also grateful to Sean Andrews and Joel Kastner for their fruitful
comments. This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2013.1.01397.S and ADS/JAO.ALMA#2011.0.00340.S. ALMA is a
partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada), NSC, ASIAA (Taiwan), and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work
is partially supported by Grants-in-Aid for Scientific Research
23103005, 25108004, 25400229, and 15H03646. T.T. was supported by JSPS
KAKENHI grant No. 23103004. C.W. is supported by the Netherlands
Organisation for Scientific Research (program number 639.041.335).
Astrophysics at QUB is supported by a grant from the STFC.
NR 35
TC 15
Z9 15
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2016
VL 819
IS 1
AR L7
DI 10.3847/2041-8205/819/1/L7
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF0QO
UT WOS:000371044200007
ER
PT J
AU Zeng, ZC
Chen, B
Ji, HS
Goode, PR
Cao, WD
AF Zeng, Zhicheng
Chen, Bin
Ji, Haisheng
Goode, Philip R.
Cao, Wenda
TI RESOLVING THE FAN-SPINE RECONNECTION GEOMETRY OF A SMALL-SCALE
CHROMOSPHERIC JET EVENT WITH THE NEW SOLAR TELESCOPE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: corona
ID X-RAY TELESCOPE; DYNAMICS-OBSERVATORY SDO; FLUX EMERGENCE; EMERGING
FLUX; MAGNETIC-FLUX; CORONAL HOLES; ANEMONE JETS; HINODE; FIELD;
SIMULATIONS
AB Jets are ubiquitously present in both quiet and active regions on the Sun. They are widely believed to be driven by magnetic reconnection. A fan-spine structure has been frequently reported in some coronal jets and flares, and has been regarded as a signature of ongoing magnetic reconnection in a topology consisting of a magnetic null connected by a fan-like separatrix surface and a spine. However, for small-scale chromospheric jets, clear evidence of such structures is rather rare, although it has been implied in earlier works that showed an inverted-Y-shaped feature. Here we report high-resolution (0 16) observations of a small-scale chromospheric jet obtained by the New Solar Telescope (NST) using 10830 angstrom filtergrams. Bi-directional flows were observed across the separatrix regions in the 10830 angstrom images, suggesting that the jet was produced due to magnetic reconnection. At the base of the jet, a fan-spine structure was clearly resolved by the NST, including the spine and the fan-like surface, as well as the loops before and after the reconnection. A major part of this fan-spine structure, with the exception of its bright footpoints and part of the base arc, was invisible in the extreme ultraviolet and soft X-ray images (observed by the Atmosphere Imaging Assembly and the X-Ray Telescope, respectively), indicating that the reconnection occurred in the upper chromosphere. Our observations suggest that the evolution of this chromospheric jet is consistent with a two-step reconnection scenario proposed by Torok et al.
C1 [Zeng, Zhicheng; Chen, Bin; Goode, Philip R.; Cao, Wenda] New Jersey Inst Technol, Ctr Solar Terr Res, 323 Martin Luther King Blvd, Newark, NJ 07102 USA.
[Zeng, Zhicheng; Ji, Haisheng; Goode, Philip R.; Cao, Wenda] Big Bear Solar Observ, 40386 North Shore Lane, Big Bear City, CA 92314 USA.
[Chen, Bin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Ji, Haisheng] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China.
RP Zeng, ZC (reprint author), New Jersey Inst Technol, Ctr Solar Terr Res, 323 Martin Luther King Blvd, Newark, NJ 07102 USA.; Zeng, ZC (reprint author), Big Bear Solar Observ, 40386 North Shore Lane, Big Bear City, CA 92314 USA.
FU NJIT; US NSF [AGS-1250818, AGS-0847126, NSFC-11333009, NSFC-11428309];
NASA [NNX13AG14G]; Korea Astronomy and Space Science Institute; Seoul
National University; strategic priority research program of CAS
[XDB09000000]; AFOSR [FA 9550-15-1-0322]; NASA from Lockheed-Martin
[SP02H1701R, NNM07AB07C]
FX The BBSO operation is supported by NJIT, US NSF AGS-1250818, and NASA
NNX13AG14G grants. The NST operation is partly supported by the Korea
Astronomy and Space Science Institute, Seoul National University, and
the strategic priority research program of CAS with grant No.
XDB09000000. We thank Antonia Savcheva and Hui Tian for helpful
discussions. We acknowledge the support of the US NSF AGS-0847126,
NSFC-11333009, NSFC-11428309, AFOSR (FA 9550-15-1-0322), and NASA under
contract SP02H1701R from Lockheed-Martin to SAO, and contract NNM07AB07C
to SAO.
NR 34
TC 3
Z9 3
U1 8
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2016
VL 819
IS 1
AR L3
DI 10.3847/2041-8205/819/1/L3
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF0QO
UT WOS:000371044200003
ER
PT J
AU Campbell, JE
Fisch, J
Langdon, C
Paul, VJ
AF Campbell, Justin E.
Fisch, Jay
Langdon, Chris
Paul, Valerie J.
TI Increased temperature mitigates the effects of ocean acidification in
calcified green algae (Halimeda spp.)
SO CORAL REEFS
LA English
DT Article
ID GREAT-BARRIER-REEF; DECLINING CORAL CALCIFICATION;
LITHOTHAMNION-CORALLIOIDES; LIGHT AVAILABILITY; PARTIAL-PRESSURE;
CARBONIC-ACID; LOW-PH; GROWTH; PHOTOSYNTHESIS; NUTRIENT
AB The singular and interactive effects of ocean acidification and temperature on the physiology of calcified green algae (Halimeda incrassata, H. opuntia, and H. simulans) were investigated in a fully factorial, 4-week mesocosm experiment. Individual aquaria replicated treatment combinations of two pH levels (7.6 and 8.0) and two temperatures (28 and 31 A degrees C). Rates of photosynthesis, respiration, and calcification were measured for all species both prior to and after treatment exposure. Pre-treatment measurements revealed that H. incrassata displayed higher biomass-normalized rates of photosynthesis and calcification (by 55 and 81 %, respectively) relative to H. simulans and H. opuntia. Furthermore, prior to treatment exposure, photosynthesis was positively correlated to calcification, suggesting that the latter process may be controlled by photosynthetic activity in this group. After treatment exposure, net photosynthesis was unaltered by pH, yet significantly increased with elevated temperature by 58, 38, and 37 % for H. incrassata, H. simulans, and H. opuntia, respectively. Both pH and temperature influenced calcification, but in opposing directions. On average, calcification declined by 41 % in response to pH reduction, but increased by 49 % in response to elevated temperature. Within each pH treatment, elevated temperature increased calcification by 23 % (at pH 8.0) and 74 % (at pH 7.6). Interactions between pH, temperature, and/or species were not observed. This work demonstrates that, in contrast to prior studies, increased temperature may serve to enhance the metabolic performance (photosynthesis and calcification) of some marine calcifiers, despite elevated carbon dioxide concentrations. Thus, in certain cases, ocean warming may mitigate the negative effects of acidification.
C1 [Campbell, Justin E.; Paul, Valerie J.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
[Fisch, Jay; Langdon, Chris] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Corals & Climate Change Lab, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
RP Campbell, JE (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM campbellju@si.edu
FU Smithsonian Hunterdon Oceanographic Endowment; Competitive Grants
Program for Science
FX We thank Lane Johnston for assistance in the laboratory. This work was
made possible through support from the Smithsonian Hunterdon
Oceanographic Endowment and the Competitive Grants Program for Science.
This is contribution no. 1013 from the Smithsonian Marine Station at
Fort Pierce, FL.
NR 66
TC 2
Z9 2
U1 10
U2 42
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
EI 1432-0975
J9 CORAL REEFS
JI Coral Reefs
PD MAR
PY 2016
VL 35
IS 1
BP 357
EP 368
DI 10.1007/s00338-015-1377-9
PG 12
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DE9KE
UT WOS:000370955100036
ER
PT J
AU Frias-Torres, S
O'Neill, MP
AF Frias-Torres, S.
O'Neill, M. P.
TI First observation of spawning of goliath grouper, Epinephelus itajara
(Retracted Article)
SO CORAL REEFS
LA English
DT Correction; Retracted Publication
C1 [Frias-Torres, S.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
[O'Neill, M. P.] Palm Beach Gardens, POB 32909, Palm Beach Gardens, FL 33420 USA.
RP Frias-Torres, S (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM sfriastorres@gmail.com
NR 1
TC 0
Z9 0
U1 3
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
EI 1432-0975
J9 CORAL REEFS
JI Coral Reefs
PD MAR
PY 2016
VL 35
IS 1
BP 369
EP 369
DI 10.1007/s00338-015-1257-3
PG 1
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DE9KE
UT WOS:000370955100037
ER
PT J
AU Griffith, AB
Salguero-Gomez, R
Merow, C
McMahon, S
AF Griffith, Alden B.
Salguero-Gomez, Roberto
Merow, Cory
McMahon, Sean
TI Demography beyond the population
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE animal population ecology; comparative biology; demography;
eco-evolutionary dynamics; functional traits; infectious diseases;
integral projection models; matrix population models; plant population
and community dynamics; range dynamics
ID INTEGRAL PROJECTION MODELS; FUNCTIONAL TRAITS; LIFE-HISTORY;
PLANT-POPULATIONS; MATRIX MODELS; DENSITY-DEPENDENCE; WOLF POPULATION;
PRACTICAL GUIDE; R-PACKAGE; DYNAMICS
AB Population ecology, the discipline that studies the dynamics of species' populations and how they interact with the environment, has been one of the most prolific fields of ecology and evolution. Demographic research is central to quantifying population-level processes and their underlying mechanisms and has provided critical contributions to a diversity of research fields. Examples include the spread of infectious diseases, eco-evolutionary dynamics and rapid evolution, mechanisms underlying invasions and extinctions, and forest productivity. As the fates of individual organisms are influenced by, and subsequently underlie, many other patterns and processes, we suggest that connecting demography beyond the population level offers promising avenues of innovation in ecology and evolution. Under the premise that population-level processes are an ideal common currency within ecology and evolution, we organized the British Ecological Society Symposium, Demography Beyond the Population. This event attracted international researchers who are applying demographic theory and approaches to a broad range of questions. This special feature builds off of the symposium and illustrates the ability of demography to connect across diverse research areas in ecology and evolution, including functional traits, transient dynamics, quantitative genetics, environmental drivers and feedbacks, land management and other topics. In addition to highlighting the contributed manuscripts, this editorial provides a brief background on the development of the discipline and suggests how demographic tools may be used in novel ways to study more than just populations.Synthesis. This special feature integrates novel lines of research in the vast field of demography that directly interact with other ecological and evolutionary disciplines. The cross-disciplinary potential of demography is further emphasized by the fact that its 20 manuscripts are spread across all six journals of the British Ecological Society. Together, these articles highlight that there is much to be gained by linking demography to other disciplines and scales in ecology and evolution.
C1 [Griffith, Alden B.] Wellesley Coll, Environm Studies Program, 106 Cent St, Wellesley, MA 02481 USA.
[Salguero-Gomez, Roberto] Univ Queensland, Sch Biol Sci, ARC Ctr Excellence Environm Decis, Brisbane, Qld 4072, Australia.
[Salguero-Gomez, Roberto] Max Planck Inst Demog Res, Evolutionary Biodemog Lab, Konrad Zuse Str 1, DE-18057 Rostock 16, Germany.
[Merow, Cory] Univ Connecticut, Dept Ecol & Evolutionary Biol, 75 North Eagleville Rd, Storrs, CT 06269 USA.
[McMahon, Sean] Smithsonian Environm Res Ctr, P647 Contees Wharf Rd, Edgewater, MD 21037 USA.
RP Griffith, AB (reprint author), Wellesley Coll, Environm Studies Program, 106 Cent St, Wellesley, MA 02481 USA.; Salguero-Gomez, R (reprint author), Univ Queensland, Sch Biol Sci, ARC Ctr Excellence Environm Decis, Brisbane, Qld 4072, Australia.; Salguero-Gomez, R (reprint author), Max Planck Inst Demog Res, Evolutionary Biodemog Lab, Konrad Zuse Str 1, DE-18057 Rostock 16, Germany.
EM agriffit@wellesley.edu; r.salguero@uq.edu.au
RI Salguero-Gomez, Roberto/N-6016-2016
OI Salguero-Gomez, Roberto/0000-0002-6085-4433
FU British Ecological Society; Wellesley College; Australian Research
Council [DE140100505]; Max Planck Institute for Demographic Research;
USDA-NRI [2008-35615-19014]; NSF [CHN 1414108, DEB-1137366]
FX We are grateful to the British Ecological Society for their support
during the organization of the symposium 'Demography Beyond the
Population' (especially to A. Simpson, A. Everard and R. English), and
the special feature (especially to A. Baier and L. Sandhu). Many thanks
are also due to the over 40 anonymous referees involved in this special
feature. J. Vaupel provided useful comments on earlier drafts of this
manuscript. A.B.G. was supported by Wellesley College. R. S-G. was
supported by the Australian Research Council (DE140100505) and by the
Max Planck Institute for Demographic Research. C.M. was supported by
USDA-NRI 2008-35615-19014 and NSF CHN 1414108. C.M. and S.M. were
supported by NSF DEB-1137366.
NR 125
TC 13
Z9 13
U1 45
U2 124
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
EI 1365-2745
J9 J ECOL
JI J. Ecol.
PD MAR
PY 2016
VL 104
IS 2
BP 271
EP 280
DI 10.1111/1365-2745.12547
PG 10
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA DE9LU
UT WOS:000370959800001
ER
PT J
AU Needham, J
Merow, C
Butt, N
Malhi, Y
Marthews, TR
Morecroft, M
McMahon, SM
AF Needham, Jessica
Merow, Cory
Butt, Nathalie
Malhi, Yadvinder
Marthews, Toby R.
Morecroft, Michael
McMahon, Sean M.
TI Forest community response to invasive pathogens: the case of ash dieback
in a British woodland
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE Bayesian inference; disease disturbance; forest demography;
individual-based models; integral projection models; inverse models;
plant population and community dynamics
ID FRAXINUS-EXCELSIOR POPULATIONS; HYMENOSCYPHUS-PSEUDOALBIDUS;
ACER-PSEUDOPLATANUS; TROPICAL FOREST; BOREAL FOREST; WYTHAM-WOODS;
DYNAMICS; GROWTH; SUCCESSION; ECOLOGY
AB Large-scale mortality events in forests are increasing in frequency and intensity and can lead to both intermediate- and long-term changes in these systems. Specialist pests and pathogens are unique disturbances, as they commonly target individual species that are relatively prevalent in the community. Understanding the consequences of pathogen-caused mortality requires using sometimes limited available data to create statistical models that can forecast future community states. In the last two decades, ash dieback disease has swept through Europe causing widespread mortality of Fraxinus excelsior L. (European ash) across much of its distribution. In the UK, F.excelsior is an abundant and ecologically important species. Using demographic data from an 18ha plot in Wytham Woods, Oxfordshire, we built models that forecast the response of this forest plot to the loss of F.excelsior. We combine integral projection models and individual-based models to link models of growth, survival and fecundity to population dynamics. We demonstrate likely responses in Wytham by comparing projections under different levels of F.excelsior mortality. To extrapolate results to other systems, we test hypotheses regarding the role of abundance, spatial structure and demographic differences between species in determining community response to disease disturbance. We show that the outcome of succession is determined largely by the differing demographic strategies and starting abundances of competing species. Spatial associations between species were shown to have little effect on community dynamics at the spatial scale of this plot.Synthesis. Host-specific pests and pathogens are an increasingly important type of disturbance. We have developed a framework that makes use of forest inventory data to forecast changes in the population dynamics of remaining species and the consequences for community structure. We use our framework to predict how a typical British woodland will respond to ash dieback disease and show how vital rates, spatial structure and abundance impact the community response to the loss of a key species.
C1 [Needham, Jessica] Univ Oxford, Dept Plant Sci, S Parks Rd, Oxford OX1 3RB, England.
[Merow, Cory] Univ Connecticut, Ecol & Evolutionary Biol, Unit 3043, 75 N Eagleville Rd, Storrs, CT 06268 USA.
[Butt, Nathalie] Univ Queensland, Sch Biol Sci, ARC Ctr Excellence Environm Decis, St Lucia, Qld 4072, Australia.
[Malhi, Yadvinder; Marthews, Toby R.] Univ Oxford, Environm Change Inst, Sch Geog & Environm, S Parks Rd, Oxford OX1 3QY, England.
[Morecroft, Michael] Nat England, Cromwell House,15 Andover Rd, Winchester SO23 7BT, Hants, England.
[McMahon, Sean M.] Smithsonian Environm Res Ctr, Smithsonian Inst Forest Global Earth Observ, 647 Contees Wharf Rd, Edgewater, MD 21307 USA.
RP Needham, J (reprint author), Univ Oxford, Dept Plant Sci, S Parks Rd, Oxford OX1 3RB, England.
EM jessica.needham@plants.ox.ac.uk
FU Department of Plant Sciences, Oxford; USA National Science Foundation
(NSF) [640261]; Clarendon Scholarship; New College Scholarship; BBSRC
FX The 18-ha Long-Term Forest Monitoring Plot is a collaborative project
between the University of Oxford, the Centre for Ecology and Hydrology,
and the Smithsonian Institution CTFS Forest-GEO (HSBC Climate
Partnership). Thanks go to Prof. Hal Caswell for assistance with the
megamatrix construction. Much of the early work on this project was
carried out at a CTFS Forest-GEO meeting for which JN received a travel
grant from the Department of Plant Sciences, Oxford. SMM and CM were
partially funded by the USA National Science Foundation (NSF 640261 to
SMM). This work forms part of JN's DPhil which is funded by a Clarendon
Scholarship, a New College Scholarship and the BBSRC. JN would like to
give special thanks to Dr. Roosa Leimu-Brown, Dr. Charlotte Metcalf and
Dr. Nick Brown for their valuable supervisory support throughout her
DPhil. The authors declare no conflict of interests.
NR 73
TC 3
Z9 3
U1 22
U2 62
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
EI 1365-2745
J9 J ECOL
JI J. Ecol.
PD MAR
PY 2016
VL 104
IS 2
BP 315
EP 330
DI 10.1111/1365-2745.12545
PG 16
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA DE9LU
UT WOS:000370959800005
ER
PT J
AU Spasojevic, MJ
Turner, BL
Myers, JA
AF Spasojevic, Marko J.
Turner, Benjamin L.
Myers, Jonathan A.
TI When does intraspecific trait variation contribute to functional
beta-diversity?
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE community assembly; determinants of plant community diversity and
structure; environmental filtering; functional diversity; Ozark
oak-hickory forest; plant functional traits; spatial scale; species
sorting; Tyson Research Center Plot
ID TROPICAL TREE COMMUNITY; ASSEMBLY PROCESSES; SPECIES-DIVERSITY;
DISTANCE-DECAY; LEAF-AREA; ECOLOGY; PLANT; VARIABILITY; PATTERNS;
FRAMEWORK
AB Intraspecific trait variation (ITV) is hypothesized to play an important role in community assembly and the maintenance of biodiversity. However, fundamental gaps remain in our understanding of how ITV contributes to mechanisms that create spatial variation in the functional-trait composition of communities (functional -diversity). Importantly, ITV may influence the perceived importance of environmental filtering across spatial scales. We examined how ITV contributes to functional -diversity and environmental filtering in woody plant communities in a temperate forest in the Ozark ecoregion, Missouri, USA. To test the hypothesis that ITV contributes to changes in the perceived importance of environmental filtering across scales, we compared patterns of functional -diversity across soil-resource and topographic gradients at three spatial grains and three spatial extents. To quantify the contribution of ITV to functional -diversity, we compared patterns that included ITV in five traits (leaf area, specific leaf area, leaf water content, leaf toughness and chlorophyll content) to patterns based on species-mean trait values. Functional -diversity that included ITV increased with spatial extent and decreased with spatial grain, suggesting stronger environmental filtering within spatially extensive landscapes that contain populations locally adapted to different habitats. In contrast, functional -diversity based on species-mean trait values increased with spatial extent but did not change with spatial grain, suggesting weaker environmental filtering among larger communities which each contain a variety of habitats and locally adapted populations.Synthesis. Although studies typically infer community assembly mechanisms from species-mean trait values, our study suggests that mean trait values may mask the strength of assembly mechanisms such as environmental filtering, especially in landscape-scale studies that encompass strong environmental gradients and locally adapted populations. Our study highlights the utility of integrating ITV into studies of functional -diversity to better understand the ecological conditions under which trait variation within and among species contributes most strongly to patterns of biodiversity across spatial scales.
C1 [Spasojevic, Marko J.; Myers, Jonathan A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA.
[Spasojevic, Marko J.; Myers, Jonathan A.] Washington Univ, Tyson Res Ctr, St Louis, MO 63130 USA.
[Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
RP Spasojevic, MJ (reprint author), Washington Univ, Dept Biol, St Louis, MO 63130 USA.; Spasojevic, MJ (reprint author), Washington Univ, Tyson Res Ctr, St Louis, MO 63130 USA.
EM mspaso@gmail.com
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
FU International Center for Advanced Renewable Energy and Sustainability
(I-CARES) at Washington University in St. Louis; National Science
Foundation [DEB 1144084, DEB 1256788]; Smithsonian Center for Tropical
Forest Science and Forest Global Earth Observatories (CTFS-ForestGEO)
Grants Program; Tyson Research Center
FX We thank Dev Harrington, Claudia Stein, Jacqueline Treiger, Maranda
Walton, Micaela Hyams and the Tyson Environmental Research Fellowship
(TERF) programme for high-school students for assistance with field and
laboratory work. We thank Jim Dalling for assistance with soil-sampling
protocols, Claire Baldeck for kriging soil variables and Francis Baum
for assistance with topographic analyses. We thank Chris Catano, Dilys
Vela, and Emma Moran for helpful comments on early drafts of the
manuscript. Financial support was provided by the International Center
for Advanced Renewable Energy and Sustainability (I-CARES) at Washington
University in St. Louis, the National Science Foundation (DEB 1144084;
DEB 1256788), the Smithsonian Center for Tropical Forest Science and
Forest Global Earth Observatories (CTFS-ForestGEO) Grants Program, and
the Tyson Research Center.
NR 56
TC 1
Z9 1
U1 15
U2 51
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
EI 1365-2745
J9 J ECOL
JI J. Ecol.
PD MAR
PY 2016
VL 104
IS 2
BP 487
EP 496
DI 10.1111/1365-2745.12518
PG 10
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA DE9LU
UT WOS:000370959800020
ER
PT J
AU Baker, TR
Diaz, DMV
Chama Moscoso, V
Navarro, G
Monteagudo, A
Pinto, R
Cangani, K
Fyllas, NM
Gonzalez, GL
Laurance, WF
Lewis, SL
Lloyd, J
ter Steege, H
Terborgh, JW
Phillips, OL
AF Baker, Timothy R.
Diaz, Dilys M. Vela
Chama Moscoso, Victor
Navarro, Gilberto
Monteagudo, Abel
Pinto, Ruy
Cangani, Katia
Fyllas, Nikolaos M.
Gonzalez, Gabriela Lopez
Laurance, William F.
Lewis, Simon L.
Lloyd, Jonathan
ter Steege, Hans
Terborgh, John W.
Phillips, Oliver L.
TI Consistent, small effects of treefall disturbances on the composition
and diversity of four Amazonian forests
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE alpha-diversity; beta-diversity; determinants of plant community
diversity and structure; functional composition; maximum height; seed
mass; tropical forest; wood density
ID TROPICAL RAIN-FORESTS; BASIN-WIDE VARIATIONS; INTERMEDIATE DISTURBANCE;
RECRUITMENT LIMITATION; SPECIES-DIVERSITY; GAP DISTURBANCES; TREES;
HYPOTHESIS; DYNAMICS; BIODIVERSITY
AB Understanding the resilience of moist tropical forests to treefall disturbance events is important for understanding the mechanisms that underlie species coexistence and for predicting the future composition of these ecosystems. Here, we test whether variation in the functional composition of Amazonian forests determines their resilience to disturbance. We studied the legacy of natural treefall disturbance events in four forests across Amazonia that differ substantially in functional composition. We compared the composition and diversity of all free-standing woody stems 2-10cm diameter in previously disturbed and undisturbed 20x20m subplots within 55, one-hectare, long-term forest inventory plots. Overall, stem number increased following disturbance, and species and functional composition shifted to favour light-wooded, small-seeded taxa. Alpha-diversity increased, but beta-diversity was unaffected by disturbance, in all four forests. Changes in response to disturbance in both functional composition and alpha-diversity were, however, small (2 - 4% depending on the parameter) and similar among forests.Synthesis. This study demonstrates that variation in the functional composition of Amazonian forests does not lead to large differences in the response of these forests to treefall disturbances, and overall, these events have a minor role in maintaining the diversity of these ecosystems.
C1 [Baker, Timothy R.; Gonzalez, Gabriela Lopez; Lewis, Simon L.; Phillips, Oliver L.] Univ Leeds, Sch Geog, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England.
[Diaz, Dilys M. Vela] Washington Univ, Dept Biol, St Louis, MO 63130 USA.
[Chama Moscoso, Victor] Univ San Antonio Abad del Cusco, Ave Cultura, Cuzco, Peru.
[Navarro, Gilberto] Univ Nacl Amazonia Peruana, Sargento Lores 385, Iquitos, Peru.
[Monteagudo, Abel] Prolongac Bolognesi Mz-E-6, Pasco, Peru.
[Pinto, Ruy; Cangani, Katia; Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia.
[Fyllas, Nikolaos M.] Univ Athens, Fac Biol, Dept Ecol & Systemat, Athens 15701, Greece.
[Laurance, William F.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, Ave Andre Araujo 2936, Manaus, Brazil.
[Laurance, William F.] Smithsonian Trop Res Inst, Ave Andre Araujo 2936, Manaus, Brazil.
[Lewis, Simon L.] UCL, Gower St, London WC1E 6BT, England.
[Lloyd, Jonathan] Univ London Imperial Coll Sci Technol & Med, Silwood Pk Campus, Ascot West SL5 7PY, Berks, England.
[ter Steege, Hans] Naturalis Biodivers Ctr, POB 9517, NL-2300 RA Leiden, Netherlands.
[Terborgh, John W.] Duke Univ, Nicholas Sch Environm, Ctr Trop Conservat, Box 90328, Durham, NC 27708 USA.
RP Baker, TR (reprint author), Univ Leeds, Sch Geog, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England.
EM t.r.baker@leeds.ac.uk
RI Phillips, Oliver/A-1523-2011; ter Steege, Amaz/B-5866-2011; Lloyd,
Jonathan/F-8893-2010;
OI Phillips, Oliver/0000-0002-8993-6168; ter Steege,
Amaz/0000-0002-8738-2659; Lloyd, Jonathan/0000-0002-5458-9960; Lewis,
Simon/0000-0002-8066-6851; Fyllas, Nikolaos/0000-0002-5651-5578
FU NERC [NE/C517484/1]; CNRS Nouragues Research Grants Program; Gordon and
Betty Moore Foundation; NERC; NGS; Biological Dynamics of Forest
Fragments Project technical series [682]
FX This work was carried out with funding from a NERC fellowship to TRB
(NE/C517484/1) and the CNRS Nouragues Research Grants Program. Database
management was funded by the Gordon and Betty Moore Foundation's support
of RAINFOR, via a grant led by Oliver Phillips. We thank CNPq (Brazil)
and SERNANPE (Peru) for research permits. Previous censuses that
contributed to the plot inventory data analysed included those funded by
NERC and NGS grants to Oliver Phillips (S Peru, N Peru). We are also
extremely grateful for the assistance of the many individuals who
provided plot data, assisted with the creation and maintenance of the
plot data base, contributed to organizing fieldwork, assisted with
identification or commented on this manuscript: Jean-Paul LaTorre, Luis
Valenzuela, Henrik Baslev, Rodolfo Vasquez, Norma Salinas, Javier Silva
Espejo, David Greenberg, Sue Grahame, Susan Laurance, Fredy Ramirez,
Regina Luizao, Henrique Nascimento, Ana Andrade, Jerome Chave, Patrick
Gaucher, Tomas Delarboulas and Patrick Chatelet. This is publication
number 682 in the Biological Dynamics of Forest Fragments Project
technical series.
NR 59
TC 0
Z9 0
U1 7
U2 36
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
EI 1365-2745
J9 J ECOL
JI J. Ecol.
PD MAR
PY 2016
VL 104
IS 2
BP 497
EP 506
DI 10.1111/1365-2745.12529
PG 10
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA DE9LU
UT WOS:000370959800021
ER
PT J
AU Nelsen, MP
DiMichele, WA
Peters, SE
Boyce, CK
AF Nelsen, Matthew P.
DiMichele, William A.
Peters, Shanan E.
Boyce, C. Kevin
TI Delayed fungal evolution did not cause the Paleozoic peak in coal
production
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE lignin; carbon cycle; wood rot; fungi; lignin degradation
ID CENTRAL APPALACHIAN BASIN; GRAND-CROIX CHERTS; AGE HERRIN COAL;
WOOD-DECAY; LIGNIN DEGRADATION; PALEOCLIMATE CONTROLS; CLAMP
CONNECTIONS; FORMING PLANTS; CENTRAL FRANCE; CARBON-CYCLE
AB Organic carbon burial plays a critical role in Earth systems, influencing atmospheric O-2 and CO2 concentrations and, thereby, climate. The Carboniferous Period of the Paleozoic is so named for massive, widespread coal deposits. A widely accepted explanation for this peak in coal production is a temporal lag between the evolution of abundant lignin production in woody plants and the subsequent evolution of lignin-degrading Agaricomycetes fungi, resulting in a period when vast amounts of lignin-rich plant material accumulated. Here, we reject this evolutionary lag hypothesis, based on assessment of phylogenomic, geochemical, paleontological, and stratigraphic evidence. Lignin-degrading Agaricomycetes may have been present before the Carboniferous, and lignin degradation was likely never restricted to them and their class II peroxidases, because lignin modification is known to occur via other enzymatic mechanisms in other fungal and bacterial lineages. Furthermore, a large proportion of Carboniferous coal horizons are dominated by unlignified lycopsid periderm with equivalent coal accumulation rates continuing through several transitions between floral dominance by lignin-poor lycopsids and lignin-rich tree ferns and seed plants. Thus, biochemical composition had little relevance to coal accumulation. Throughout the fossil record, evidence of decay is pervasive in all organic matter exposed subaerially during deposition, and high coal accumulation rates have continued to the present wherever environmental conditions permit. Rather than a consequence of a temporal decoupling of evolutionary innovations between fungi and plants, Paleozoic coal abundance was likely the result of a unique combination of everwet tropical conditions and extensive depositional systems during the assembly of Pangea.
C1 [Nelsen, Matthew P.; Boyce, C. Kevin] Stanford Univ, Geol Sci, Stanford, CA 94305 USA.
[DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
[Peters, Shanan E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
RP Boyce, CK (reprint author), Stanford Univ, Geol Sci, Stanford, CA 94305 USA.
EM ckboyce@stanford.edu
RI Peters, Shanan/A-5620-2013
OI Peters, Shanan/0000-0002-3346-4317
FU National Science Foundation [EAR-1150082]; Stanford University School of
Earth, Energy & Environmental Sciences
FX Discussion and comments from A. Baresch, K. Larson-Johnson, J. Payne,
and two anonymous reviewers improved the manuscript. We thank S. Smith
for collections and photographic assistance, K. Peay, M. Nelsen, and P.
Nelsen for providing material for Fig. 2A, and the Smithsonian National
Museum of Natural History and the University of Michigan Museum of
Paleontology for specimen access. M.P.N. and C.K.B. acknowledge the
Stanford University School of Earth, Energy & Environmental Sciences for
support, and S.E.P. acknowledges support from National Science
Foundation EAR-1150082.
NR 138
TC 5
Z9 5
U1 10
U2 26
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAR 1
PY 2016
VL 113
IS 9
BP 2442
EP 2447
DI 10.1073/pnas.1517943113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF2WG
UT WOS:000371204500050
PM 26787881
ER
PT J
AU Rose, A
Kolar, M
Tschapka, M
Knornschild, M
AF Rose, Andreas
Kolar, Miriam
Tschapka, Marco
Knornschild, Mirjam
TI Learning where to feed: the use of social information in flower-visiting
Pallas' long-tongued bats (Glossophaga soricina)
SO ANIMAL COGNITION
LA English
DT Article
DE Chiroptera; Demonstrator-observer paradigm; Local enhancement; Social
facilitation; Social transmission; Spatial memory
ID LOWLAND RAIN-FOREST; FORAGING BEHAVIOR; FOOD; TRANSMISSION; MEMORY;
CALLS; FACILITATION; ENVIRONMENT; VERTEBRATES; CHIROPTERA
AB Social learning is a widespread phenomenon among vertebrates that influences various patterns of behaviour and is often reported with respect to foraging behaviour. The use of social information by foraging bats was documented in insectivorous, carnivorous and frugivorous species, but there are little data whether flower-visiting nectarivorous bats (Phyllostomidae: Glossophaginae) can acquire information about food from other individuals. In this study, we conducted an experiment with a demonstrator-observer paradigm to investigate whether flower-visiting Pallas' long-tongued bats (Glossophaga soricina) are able to socially learn novel flower positions via observation of, or interaction with, knowledgeable conspecifics. The results demonstrate that flower-visiting G. soricina are able to use social information for the location of novel flower positions and can thereby reduce energy-costly search efforts. This social transmission is explainable as a result of local enhancement; learning bats might rely on both visual and echo-acoustical perception and are likely to eavesdrop on auditory cues that are emitted by feeding conspecifics. We additionally tested the spatial memory capacity of former demonstrator bats when retrieving a learned flower position, and the results indicate that flower-visiting bats remember a learned flower position after several weeks.
C1 [Rose, Andreas; Kolar, Miriam; Tschapka, Marco; Knornschild, Mirjam] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Helmholtzstr 10-1, D-89069 Ulm, Germany.
[Tschapka, Marco; Knornschild, Mirjam] Smithsonian Trop Res Inst, Roosevelt Ave,Tupper Bldg 401, Balboa, Panama.
RP Rose, A (reprint author), Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Helmholtzstr 10-1, D-89069 Ulm, Germany.
EM andreas.rose@uni-ulm.de
FU German Baden-Wurttemberg Stiftung, Eliteprogramme for Postdocs
FX We thank Ulrike Stehle and Sebastian Zschunke for maintenance of the bat
colonies, for providing technical equipment and for their general
helpfulness. We thank Maria Eckenweber and Patrick Cvecko for fruitful
discussions and critical comments on the manuscript. We further thank
Dr. Cheng, Dr. Nachev and one anonymous reviewer for their time and
helpful suggestions. This work was supported by the German
Baden-Wurttemberg Stiftung, Eliteprogramme for Postdocs (M.K.).
NR 49
TC 0
Z9 0
U1 9
U2 32
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1435-9448
EI 1435-9456
J9 ANIM COGN
JI Anim. Cogn.
PD MAR
PY 2016
VL 19
IS 2
BP 251
EP 262
DI 10.1007/s10071-015-0930-9
PG 12
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA DD8IQ
UT WOS:000370170300001
PM 26497984
ER
PT J
AU Uribe, MC
Grier, HJ
De la Rosa-Cruz, G
Schartl, M
AF Carmen Uribe, Mari
Grier, Harry J.
De la Rosa-Cruz, Gabino
Schartl, Manfred
TI The occurrence of spermatozoa in the ovary of the gynogenetic viviparous
teleost Poecilia formosa (POECILIIDAE)
SO JOURNAL OF MORPHOLOGY
LA English
DT Article
DE parthenogenesis; gynogenesis; oogenesis; intraovarian gestation;
embryonic development; ovarian histology
ID FINE-STRUCTURE; ORIGIN; FISH; RETICULATA; STORAGE; HYBRID
AB The reproductive mode of the female viviparous teleost Poecilia formosa (Poeciliidae) represents the phenomenon known as gynogenesis; that is, parthenogenetic development is initiated by spermatozoa which are needed for physiological activation of the egg and the initiation of gestation, but spermatozoa are prevented from contributing to the genome of the embryo. For the reason that no previous histological analyses of the ovary of this species during the reproductive cycle has been published the present study has been conducted. This study examined the histology of the ovary of P. formosa during nongestation and gestation phases and identified the presence of spermatozoa inside the ovary. Spermatozoa were observed in folds of the ovarian epithelium of P. formosa during both the nongestation and gestation phases. Sperm storage as documented in this study is a very important trait for the gynogenetic viviparous fish P. formosa contributing to the understanding of this species reproduction. J. Morphol. 277:341-350, 2016. (c) 2015 Wiley Periodicals, Inc.
C1 [Carmen Uribe, Mari; De la Rosa-Cruz, Gabino] Univ Nacl Autonoma Mexico, Reprod Biol Lab, Fac Ciencias, Dept Biol Comparada, Ciudad Univ, Mexico City 04510, DF, Mexico.
[Grier, Harry J.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, MRC 159, Washington, DC 20560 USA.
[Grier, Harry J.] Florida Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, St Petersburg, FL USA.
[Schartl, Manfred] Univ Wurzburgand, Comprehens Canc Ctr Mainfranken, Physiol Chem, Univ Clin Wurzburg,Bioctr, D-97074 Wurzburg, Germany.
RP Uribe, MC (reprint author), Univ Nacl Autonoma Mexico, Reprod Biol Lab, Fac Ciencias, Dept Biol Comparada, Ciudad Univ, Mexico City 04510, DF, Mexico.
EM mari3uribe3@gmail.com
OI Schartl, Manfred/0000-0001-9882-5948
NR 32
TC 0
Z9 0
U1 2
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0362-2525
EI 1097-4687
J9 J MORPHOL
JI J. Morphol.
PD MAR
PY 2016
VL 277
IS 3
BP 341
EP 350
DI 10.1002/jmor.20499
PG 10
WC Anatomy & Morphology
SC Anatomy & Morphology
GA DE4MO
UT WOS:000370603900005
PM 26680644
ER
PT J
AU Muscarella, R
Uriarte, M
Aide, TM
Erickson, DL
Forero-Montana, J
Kress, WJ
Swenson, NG
Zimmerman, JK
AF Muscarella, Robert
Uriarte, Maria
Aide, T. Mitchell
Erickson, David L.
Forero-Montana, Jimena
Kress, W. John
Swenson, Nathan G.
Zimmerman, Jess K.
TI Functional convergence and phylogenetic divergence during secondary
succession of subtropical wet forests in Puerto Rico
SO JOURNAL OF VEGETATION SCIENCE
LA English
DT Article
DE Acquisitive-conservative spectrum; Community-weighted mean traits;
Competition-colonization trade-off; Functional diversity; LMA; Maximum
height; Seed size; Successional niche hypothesis; Tropical secondary
forests; Wood density
ID TROPICAL FOREST; COMMUNITY STRUCTURE; ECONOMICS SPECTRUM; ASSEMBLY
PROCESSES; PLANT-COMMUNITIES; LAND-USE; DIVERSITY; COEXISTENCE;
DISTURBANCE; WORLDWIDE
AB QuestionUnderstanding how the relative importance of different community assembly processes changes during secondary succession of diverse systems remains elusive. Functional and phylogenetic approaches that place species along continuous axes of niche differentiation and evolutionary relatedness, however, are deepening our understanding of the mechanisms that drive successional dynamics. We ask whether successional shifts in the functional and phylogenetic composition of post-agricultural tropical forests provide evidence for niche partitioning or competitive dominance hierarchies as drivers of successional change.
LocationSubtropical wet forests, Puerto Rico.
MethodsWe combined data on four functional traits [leaf dry mass per area (LMA), wood density (WD), maximum height (H-max), seed dry mass] and a well-resolved molecular phylogeny to characterize taxonomic, functional and phylogenetic composition of sapling and adult tree communities along a regionally replicated chronosequence. We used a null model approach to assess how functional and phylogenetic diversity change with forest age.
ResultsCorresponding increases of community-weighted mean LMA, H-max and seed mass with forest age reflected a shift in dominance of species with acquisitive resource-use strategies and small seeds towards species with more conservative resource use and larger seeds. A negative relationship between forest age and local diversity of H-max and seed mass suggested increased importance of competitive hierarchies for light capture and shade-tolerant regeneration in older forests. In contrast, the colonization of palms in older forest plots led to a positive relationship between forest age and local phylogenetic diversity, suggesting functional convergence of distantly related lineages on traits that confer competitive dominance under low resource conditions.
ConclusionsWe linked both functional and phylogenetic dimensions of community diversity with successional trajectories of post-agricultural tropical forests. Contrasting patterns of these dimensions of diversity shed light on the underlying community assembly processes. We argue that integrating traits and phylogeny with specific hypotheses about physiological and historical mechanisms is essential for advancing our understanding of the drivers of community change during succession.
C1 [Muscarella, Robert; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, 10th Floor Schermerhorn Ext,1200 Amsterdam Ave, New York, NY 10027 USA.
[Muscarella, Robert] Aarhus Univ, Sect Ecoinformat & Biodivers, Ny Munkegade 116,Bldg 1540, DK-8000 Aarhus C, Denmark.
[Aide, T. Mitchell] Univ Puerto Rico, Dept Biol, POB 23360, San Juan, PR 00931 USA.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, 10th St & Constitut Ave NW, Washington, DC 20560 USA.
[Forero-Montana, Jimena; Zimmerman, Jess K.] Univ Puerto Rico, Dept Environm Sci, San Juan, PR 00925 USA.
[Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
RP Muscarella, R (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 10th Floor Schermerhorn Ext,1200 Amsterdam Ave, New York, NY 10027 USA.; Muscarella, R (reprint author), Aarhus Univ, Sect Ecoinformat & Biodivers, Ny Munkegade 116,Bldg 1540, DK-8000 Aarhus C, Denmark.
EM bob.muscarella@gmail.com; mu2126@columbia.edu; tmaide@yahoo.com;
ericksond@si.edu; jimefore@yahoo.com; kressj@si.edu; swenson@umd.edu;
jesskz@ites.upr.edu
FU NSF [DEB 1050957, DEB 1311367, DBI 1401312]; Earth Institute; Institute
of Latin American studies at Columbia University
FX We thank the landowners who generously allowed us to work on their
property. Robin Chazdon, Duncan Menge, Lourens Poorter, Jesse Lasky,
Benedicte Bachelot, Naomi Schwartz, Benjamin Taylor and several
anonymous reviewers provided valuable comments on this manuscript. This
work was supported by NSF DEB 1050957 to MU, NSF DEB 1311367 to MU and
RM, NSF DBI 1401312 to RM, as well as grants from the Earth Institute
and Institute of Latin American studies at Columbia University.
NR 69
TC 4
Z9 4
U1 15
U2 44
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1100-9233
EI 1654-1103
J9 J VEG SCI
JI J. Veg. Sci.
PD MAR
PY 2016
VL 27
IS 2
BP 283
EP 294
DI 10.1111/jvs.12354
PG 12
WC Plant Sciences; Ecology; Forestry
SC Plant Sciences; Environmental Sciences & Ecology; Forestry
GA DE4SV
UT WOS:000370621500009
ER
PT J
AU Kersey, DC
Aitken-Palmer, C
Rivera, S
Willis, EL
Liang, LY
Snyder, RJ
AF Kersey, David C.
Aitken-Palmer, Copper
Rivera, Sam
Willis, Erin L.
Liang, Liu Yu
Snyder, Rebecca J.
TI The birth of a giant panda: Tracking the biological factors that
successfully contribute to conception through to postnatal development
SO THERIOGENOLOGY
LA English
DT Article
DE Noninvasive hormone monitoring; Giant panda; Ceruloplasmin; Fetal growth
ID AILUROPODA-MELANOLEUCA; PREGNANCY; ESTRUS; SERUM
AB Reproducing giant pandas (Ailuropoda melanoleuca) remains the most challenging aspect of managed care of this species. However, advancement in knowledge stemming from basic science research on the giant panda has facilitated a growth in the population. Here, we report the successful application of reproductive technologies, including noninvasive hormone monitoring, behavioralimorphometric observations, ultrasonographic evaluations, and acute phase protein assessment, in an individual female. By applying these approaches to one female, we report the practicality and usefulness of a multidisciplinary approach to reproductive care of the species. In addition, the utilization of various technologies across multiple physiological states also provided us an opportunity to record previously understudied events, such as maternal response to weaning and growth of a conceptus. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Kersey, David C.] Western Univ Hlth Sci, Coll Vet Med, Pomona, CA USA.
[Aitken-Palmer, Copper] Smithsonian Conservat Biol Inst, Dept Conservat Med, Front Royal, VA USA.
[Rivera, Sam; Snyder, Rebecca J.] Zoo Atlanta, Dept Anim Hlth, Atlanta, GA USA.
[Willis, Erin L.] Memphis Zool Soc, Dept Conservat & Res, Memphis, TN USA.
[Liang, Liu Yu] Chengdu Res Base Giant Panda Breeding, Chengdu, Peoples R China.
[Snyder, Rebecca J.] Oklahoma City Zoo & Bot Gardens, Dept Conservat & Sci, Oklahoma City, OK USA.
[Willis, Erin L.] Oklahoma State Univ, Dept Physiol Sci, Vet Hlth Sci Ctr, Stillwater, OK 74078 USA.
RP Kersey, DC (reprint author), Western Univ Hlth Sci, Coll Vet Med, Pomona, CA USA.
EM dkersey@westernu.edu
OI Willis, Erin/0000-0002-9234-8762
FU Zoo Atlanta
FX The authors would like to thank the Zoo Atlanta for funding the analyses
in this study and providing the animal care and keeper staff to collect
the data and samples.
NR 27
TC 0
Z9 0
U1 8
U2 27
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0093-691X
EI 1879-3231
J9 THERIOGENOLOGY
JI Theriogenology
PD MAR 1
PY 2016
VL 85
IS 4
BP 671
EP 677
DI 10.1016/j.theriogenology.2015.10.005
PG 7
WC Reproductive Biology; Veterinary Sciences
SC Reproductive Biology; Veterinary Sciences
GA DD7NN
UT WOS:000370111500013
PM 26559471
ER
PT J
AU Nganvongpanit, K
Brown, JL
Buddhachat, K
Somgird, C
Thitaram, C
AF Nganvongpanit, Korakot
Brown, Janine L.
Buddhachat, Kittisak
Somgird, Chaleamchat
Thitaram, Chatchote
TI Elemental Analysis of Asian Elephant (Elephas maximus) Teeth Using X-ray
Fluorescence and a Comparison to Other Species
SO BIOLOGICAL TRACE ELEMENT RESEARCH
LA English
DT Article
DE Tooth; Mineral; XRF; Elephant; Animal
ID MECHANICAL-PROPERTIES; LOXODONTA-AFRICANA; DECIDUOUS TEETH; BONE; IVORY;
LEAD; ENAMEL; ZINC; CONTAMINATION; CHILDREN
AB Elemental composition in bone of the different species has variation depending on genetic and environmental factors especially their food habitat. The aims of this study were to conduct an elemental analysis of Asian elephant teeth, both deciduous (first molar, second molar, and tusk) and permanent (molar and tusk), and compare the elemental composition of permanent teeth among 15 species, mostly mammalian. These teeth were analyzed using X-ray fluorescence at two voltages: 15 and 50 kV. In Asian elephants, deciduous tusk showed a lower Ca/Zn ratio compared to permanent tusk, because of the lack of Zn in permanent molars. Ca/Fe ratio was higher in deciduous than permanent molars. For permanent teeth, elephant molars presented a high Ca/Pb ratio but no Ca/Zn, Ca/Sr, and Zn/Fe ratios because of the lack of Zn and Sr in the samples tested. The key elemental ratios for differentiating elephant deciduous and permanent tusk were Ca/P and Ca/Zn. The considerable variation in elemental ratio data across 15 species was observed. All tooth samples contained Ca and P, which was not surprising; however, Pb also was present in all samples and Cd in a large majority, suggesting exposure to environmental contaminants. From discriminant analysis, the combination of Ca/P+Ca/Zn+Ca/Pb+Ca/Fe+Ca/Sr+Zn/Fe can generate two equations that successfully classified six (dog, pig, goat, tapir, monkey, and elephant) out of 15 species at 100 % specificity. In conclusion, determining the elemental profile of teeth may serve as a tool to identify the tooth "type" of elephants and to potentially classify other species.
C1 [Nganvongpanit, Korakot; Buddhachat, Kittisak] Chiang Mai Univ, Anim Bone & Joint Res Lab, Dept Vet Biosci & Publ Hlth, Fac Vet Med, Chiang Mai 50100, Thailand.
[Nganvongpanit, Korakot; Somgird, Chaleamchat; Thitaram, Chatchote] Chiang Mai Univ, Elephant Res & Educ Ctr, Fac Vet Med, Chiang Mai 50100, Thailand.
[Brown, Janine L.] Natl Zool Pk, Ctr Species Survival, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
RP Nganvongpanit, K (reprint author), Chiang Mai Univ, Anim Bone & Joint Res Lab, Dept Vet Biosci & Publ Hlth, Fac Vet Med, Chiang Mai 50100, Thailand.
EM korakot.n@cmu.ac.th; BrownJan@si.edu; k_buddhachat@yahoo.com;
nibivet@yahoo.com; cthitaram@gmail.com
FU Elephant Research and Education Center, Faculty of Veterinary Medicine,
Chiang Mai University, Chiang Mai, Thailand; Faculty of Veterinary
Medicine, Chiang Mai University, Chiang Mai, Thailand
FX The authors wish to acknowledge Miss Nutcatcher Pitakarnnop for her
diligent laboratory work. Special thanks to Dr. Patcharaporn Kaewmong,
Phuket Marine Biological Center, Thailand and Dr. Raksiri Nomsiri,
Chiang Mai Night Safari, Thailand from the Animal Anatomy Museum,
Department of Veterinary Bioscience and Public Health, Faculty of
Veterinary Medicine, Chiang Mai University for providing all samples
used in this study. The authors are also grateful for research funding
from the Elephant Research and Education Center, Faculty of Veterinary
Medicine, Chiang Mai University, Chiang Mai, Thailand and Faculty of
Veterinary Medicine, Chiang Mai University, Chiang Mai, Thailand.
NR 34
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U1 3
U2 14
PU HUMANA PRESS INC
PI TOTOWA
PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA
SN 0163-4984
EI 1559-0720
J9 BIOL TRACE ELEM RES
JI Biol. Trace Elem. Res.
PD MAR
PY 2016
VL 170
IS 1
BP 94
EP 105
DI 10.1007/s12011-015-0445-x
PG 12
WC Biochemistry & Molecular Biology; Endocrinology & Metabolism
SC Biochemistry & Molecular Biology; Endocrinology & Metabolism
GA DD5CZ
UT WOS:000369941500011
PM 26194819
ER
PT J
AU Doughty, CL
Langley, JA
Walker, WS
Feller, IC
Schaub, R
Chapman, SK
AF Doughty, Cheryl L.
Langley, J. Adam
Walker, Wayne S.
Feller, Ilka C.
Schaub, Ronald
Chapman, Samantha K.
TI Mangrove Range Expansion Rapidly Increases Coastal Wetland Carbon
Storage
SO ESTUARIES AND COASTS
LA English
DT Article
DE Climate change; Range expansion; Ecotone; Carbon storage; Mangrove; Salt
marsh
ID GULF-OF-MEXICO; SEA-LEVEL RISE; CLIMATE-CHANGE; AVICENNIA-GERMINANS;
SALT-MARSH; ECOSYSTEM SERVICES; UNITED-STATES; ELEVATED CO2; FORESTS;
IMPACTS
AB The climate change-induced expansion of mangroves into salt marshes could significantly alter the carbon (C) storage capacity of coastal wetlands, which have the highest average C storage per land area among unmanaged terrestrial ecosystems. Mangrove range expansion is occurring globally, but little is known about how these rapid climate-driven shifts may alter ecosystem C storage. Here, we quantify current C stocks in ecotonal wetlands across gradients of marsh- to mangrove-dominance, and use unique chronological maps of vegetation cover to estimate C stock changes from 2003 to 2010 in a 567-km(2) wildlife refuge in the mangrove-salt marsh ecotone. We report that over the 7-yr. period, total wetland C stocks increased 22 % due to mangrove encroachment into salt marshes. Newly established mangrove stands stored twice as much C on a per area basis as salt marsh primarily due to differences in aboveground biomass, and mangrove cover increased by 69 % during this short time interval. Wetland C storage within the wildlife refuge increased at a rate of 2.7 Mg C ha(-1) yr.(-1), more than doubling the naturally high coastal wetland C sequestration rates. Mangrove expansion could account for a globally significant increase of terrestrial C storage, which may exert a considerable negative feedback on warming.
C1 [Doughty, Cheryl L.; Langley, J. Adam; Chapman, Samantha K.] Villanova Univ, Dept Biol, 800 E Lancaster Ave, Villanova, PA 19085 USA.
[Walker, Wayne S.] Woods Hole Res Ctr, 149 Woods Hole Rd, Falmouth, MA 02540 USA.
[Feller, Ilka C.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
[Schaub, Ronald] InoMedic Hlth Applicat Inc, Mailcode IHA 300, Kennedy Space Ctr, FL 32899 USA.
RP Doughty, CL (reprint author), Villanova Univ, Dept Biol, 800 E Lancaster Ave, Villanova, PA 19085 USA.
EM cheryl.doughty@gmail.com
OI Feller, Ilka/0000-0002-6391-1608
FU National Aeronautics and Space Administration [NNX11AO94G, NNX12AF55G];
National Science Foundation [EF 1065821]; Link Graduate Fellowship at
the Smithsonian Marine Station in Fort Pierce, FL (SMSFP) [986]
FX Funding for this work was provided by grants from the National
Aeronautics and Space Administration Climate and Biological Response
Program (NNX11AO94G, NNX12AF55G) and the National Science Foundation
Macrosystems Biology Program (EF 1065821). This work was conducted as
part of NASA's Climate Adaptation Science Investigators (CASI)
Workgroup. Cheryl Doughty was also supported by a Link Graduate
Fellowship at the Smithsonian Marine Station in Fort Pierce, FL (SMSFP
Contribution No. 986). We would like to thank Glenn Coldren, Lorae
Simpson, Joseph Funk and Regina Kukola for support in field collections,
Courtney Curran and Julie Kurtz for sample preparation, and Lisa Duckett
for C:N sample analysis. We also acknowledge Jim Lyon from the U.S. Fish
and Wildlife Service, and Lynne Phillips and Carlton Hall for continued
support from the NASA Kennedy Space Center Environmental and Ecological
Programs. Lastly, we thank the editor and the two anonymous reviewers
whose suggestions have greatly improved the quality of the manuscript.
NR 74
TC 12
Z9 12
U1 20
U2 78
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
EI 1559-2731
J9 ESTUAR COAST
JI Estuaries Coasts
PD MAR
PY 2016
VL 39
IS 2
BP 385
EP 396
DI 10.1007/s12237-015-9993-8
PG 12
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA DC9GA
UT WOS:000369527900006
ER
PT J
AU Franklin, AD
Schmidt-Kuntzel, A
Terio, KA
Marker, LL
Crosier, AE
AF Franklin, Ashley D.
Schmidt-Kuentzel, Anne
Terio, Karen A.
Marker, Laurie L.
Crosier, Adrienne E.
TI Serum Amyloid A Protein Concentration in Blood is Influenced by Genetic
Differences in the Cheetah (Acinonyx jubatus)
SO JOURNAL OF HEREDITY
LA English
DT Article
DE Acute phase response; amyloidosis; cheetah; genetic typing of
insertion/deletion; serum amyloid A
ID GENERALIZED AA-AMYLOIDOSIS; ACUTE-PHASE RESPONSE; KAPPA-B-ALPHA;
INFLAMMATORY DISEASES; SYSTEMIC AMYLOIDOSIS; RENAL AMYLOIDOSIS; CATS;
ACTIVATION; PHOSPHORYLATION; POLYMORPHISM
AB Systemic amyloid A (AA) amyloidosis is a major cause of morbidity and mortality among captive cheetahs. The self-aggregating AA protein responsible for this disease is a byproduct of serum amyloid A (SAA) protein degradation. Transcriptional induction of the SAA1 gene is dependent on both C/EBP beta and NF-kappa B cis-acting elements within the promoter region. In cheetahs, 2 alleles exist for a single guanine nucleotide deletion in the putative NF-kappa B binding site. In this study, a novel genotyping assay was developed to screen for the alleles. The results show that the SAA1A(-97delG) allele is associated with decreased SAA protein concentrations in the serum of captive cheetahs (n = 58), suggesting genetic differences at this locus may be affecting AA amyloidosis prevalence. However, there was no significant difference in the frequency of the SAA1A(-97delG) allele between individuals confirmed AA amyloidosis positive versus AA amyloidosis negative at the time of necropsy (n = 48). Thus, even though there is evidence that having more copies of the SAA1A(-97delG) allele results in a potentially protective decrease in serum concentrations of SAA protein in captive cheetahs, genotype is not associated with this disease within the North American population. These results suggest that other factors are playing a more significant role in the pathogenesis of AA amyloidosis among captive cheetahs.
C1 [Franklin, Ashley D.] Univ Maryland, Dept Anim Sci, College Pk, MD 20742 USA.
[Franklin, Ashley D.; Crosier, Adrienne E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA.
[Schmidt-Kuentzel, Anne; Marker, Laurie L.] Cheetah Conservat Fund, POB 1755, Otjiwarongo, Namibia.
[Schmidt-Kuentzel, Anne] Cheetah Conservat Fund, Life Technol Conservat Genet Lab, POB 1755, Otjiwarongo, Namibia.
[Terio, Karen A.] Univ Illinois, Zool Pathol Program, Maywood, IL 60153 USA.
RP Franklin, AD (reprint author), Univ Maryland, Dept Anim Sci, College Pk, MD 20742 USA.; Franklin, AD (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM ashley.franklin@pdza.org
RI Franklin, Ashley/J-3069-2015
OI Franklin, Ashley/0000-0002-0818-5156
FU Animal Sciences Graduate Student Association (ASGSA) at the University
of Maryland College Park; Cosmos Club Foundation (Washington, DC);
Emanuel J. Friedman Philanthropies; Smithsonian Institution Fellowship
FX Animal Sciences Graduate Student Association (ASGSA) at the University
of Maryland College Park; the Cosmos Club Foundation (Washington, DC);
Emanuel J. Friedman Philanthropies; and a Smithsonian Institution
Fellowship to A.D.F.
NR 42
TC 2
Z9 2
U1 3
U2 13
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-1503
EI 1465-7333
J9 J HERED
JI J. Hered.
PD MAR
PY 2016
VL 107
IS 2
BP 115
EP 121
DI 10.1093/jhered/esv089
PG 7
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA DD6VY
UT WOS:000370063900003
PM 26585380
ER
PT J
AU Prosser, SWJ
deWaard, JR
Miller, SE
Hebert, PDN
AF Prosser, Sean W. J.
deWaard, Jeremy R.
Miller, Scott E.
Hebert, Paul D. N.
TI DNA barcodes from century-old type specimens using next-generation
sequencing
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE degraded DNA; DNA barcoding; DNA sequencing; next-generation sequencing;
type specimens
ID MINI-BARCODES; IDENTIFICATION; LEPIDOPTERA; DISSECTION; EXTRACTION;
PRIMERS; QUALITY; DAMAGE
AB Type specimens have high scientific importance because they provide the only certain connection between the application of a Linnean name and a physical specimen. Many other individuals may have been identified as a particular species, but their linkage to the taxon concept is inferential. Because type specimens are often more than a century old and have experienced conditions unfavourable for DNA preservation, success in sequence recovery has been uncertain. This study addresses this challenge by employing next-generation sequencing (NGS) to recover sequences for the barcode region of the cytochrome c oxidase 1 gene from small amounts of template DNA. DNA quality was first screened in more than 1800 century-old type specimens of Lepidoptera by attempting to recover 164-bp and 94-bp reads via Sanger sequencing. This analysis permitted the assignment of each specimen to one of three DNA quality categories - high (164-bp sequence), medium (94-bp sequence) or low (no sequence). Ten specimens from each category were subsequently analysed via a PCR-based NGS protocol requiring very little template DNA. It recovered sequence information from all specimens with average read lengths ranging from 458bp to 610bp for the three DNA categories. By sequencing ten specimens in each NGS run, costs were similar to Sanger analysis. Future increases in the number of specimens processed in each run promise substantial reductions in cost, making it possible to anticipate a future where barcode sequences are available from most type specimens.
C1 [Prosser, Sean W. J.; deWaard, Jeremy R.; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
[Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Prosser, SWJ (reprint author), Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
EM sprosser@uoguelph.ca
RI deWaard, Jeremy/G-8112-2014;
OI Miller, Scott/0000-0002-4138-1378
FU Gordon and Betty Moore Foundation; government of Canada through Genome
Canada; Ontario Genomics Institute; Ontario Ministry of Research and
Innovation; US National Institutes of Health through ICBG
[5UO1TW006671]; US National Science Foundation [DEB-0211591, 0515678]
FX This research was primarily funded by a grant to PDNH and SEM from the
Gordon and Betty Moore Foundation. Funding from the government of Canada
through Genome Canada and the Ontario Genomics Institute to the
International Barcode of Life Project also aided the work. Support from
the Ontario Ministry of Research and Innovation enabled the development
of BOLD, while the Canada Foundation for Innovation provided key
research infrastructure. Imaging and specimen lysis was supported by the
US National Institutes of Health through ICBG 5UO1TW006671 granted to
SEM. Building the Papua New Guinea background library has been supported
by the US National Science Foundation (via grants DEB-0211591, 0515678
and others to SEM). We thank the Natural History Museum and its staff
(particularly Jacqueline Mackenzie-Dodds, Geoff Martin and John Chainey)
for their support and for permitting access to type specimens. We are
grateful to David Pollock, Margaret Rosati and Jeremy Holloway who aided
tissue sampling and/or taxonomic validation. We also thank Nataly
Ivanova, Evgeny Zakharov and Sujeevan Ratnasingham who contributed to
protocol development and sequence analyses. Thermo Fisher Scientific
provided advice on protocols for the Ion Torrent platform, but did not
influence experimental design, data analysis or data interpretation.
NR 40
TC 13
Z9 13
U1 4
U2 19
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-098X
EI 1755-0998
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD MAR
PY 2016
VL 16
IS 2
BP 487
EP 497
DI 10.1111/1755-0998.12474
PG 11
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA DC3RS
UT WOS:000369137000012
PM 26426290
ER
PT J
AU Zimbelman, JR
Scheidt, SP
de Silva, SL
Bridges, NT
Spagnuolo, MG
Neely, EM
AF Zimbelman, J. R.
Scheidt, S. P.
de Silva, S. L.
Bridges, N. T.
Spagnuolo, M. G.
Neely, E. M.
TI Aerodynamic roughness height for gravel-mantled megaripples, with
implications for wind profiles near TARs on Mars
SO ICARUS
LA English
DT Article
DE Earth; Geological processes Mars; surface
ID TRANSVERSE AEOLIAN RIDGES; SURFACE-ROUGHNESS; ARGENTINEAN PUNA;
TRANSPORT; RIPPLES; DUNES; EARTH; INITIATION; DYNAMICS; MODEL
AB Aerodynamic roughness heights of 1-3 cm were obtained from measured wind profiles collected among fields of gravel-mantled megaripples in the high desert of the Puna region of northwestern Argentina. Roughness height appears to be relatively insensitive to the angle at which the wind was incident upon the bedforms throughout the study sites. The results represent the first wind profiling measurements for large megaripples, but they also demonstrate the importance of a careful evaluation of many potential effects that can influence the utility of wind profiling data. The same effects that influence collection of fieldwork data must also be considered in any prediction of wind profiles anticipated to occur near Transverse Aeolian Ridges and other aeolian features on Mars that are intermediate in scale between wind ripples and small sand dunes.
C1 [Zimbelman, J. R.; Scheidt, S. P.] Smithsonian Inst, Washington, DC 20013 USA.
[Scheidt, S. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[de Silva, S. L.; Spagnuolo, M. G.; Neely, E. M.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Bridges, N. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Spagnuolo, M. G.] UBA CONICET, IDEAN, Cuidad De Bs As, Argentina.
RP Zimbelman, JR (reprint author), Smithsonian Inst, CEPS NASM MRC 315, Washington, DC 20013 USA.
RI Bridges, Nathan/D-6341-2016; de Silva, Shanaka/A-4630-2011
OI de Silva, Shanaka/0000-0002-0310-5516
FU NASA Mars Fundamental Research Program [NNX10AP79G]; NASA Mars Data
Analysis Program [NNX12AJ38G]
FX This work was supported through a now-concluded NASA Mars Fundamental
Research Program grant (NNX10AP79G) to Oregon State University (S.L. de
Silva, P.I.), and analysis supplemented by NASA Mars Data Analysis
Program grant NNX12AJ38G (J.R. Zimbelman, P.I.). The patience of the
Editor and the comments of two anonymous reviewers were very helpful in
improving the manuscript, particularly one reviewer who patiently worked
with us through multiple iterations and brought to our attention the
important Wieringa (1993) and Marticorena et al. (2006) papers.
NR 40
TC 0
Z9 0
U1 1
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 1
PY 2016
VL 266
BP 306
EP 314
DI 10.1016/j.icarus.2015.11.008
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7DH
UT WOS:000367964300023
ER
PT J
AU Hong, J
Romaine, S
AF Hong, Jaesub
Romaine, Suzanne
CA MiXO Team
TI Miniature lightweight X-ray optics (MiXO) for surface elemental
composition mapping of asteroids and comets
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE X-ray fluorescence; Elemental abundance; X-ray imaging
ID ITOKAWA; SPECTROMETRY; TELESCOPE; PARTICLES
AB The compositions of diverse planetary bodies are of fundamental interest to planetary science, providing clues to the formation and evolutionary history of the target bodies and the solar system as a whole. Utilizing the X-ray fluorescence unique to each atomic element, X-ray imaging spectroscopy is a powerful diagnostic tool of the chemical and mineralogical compositions of diverse planetary bodies. Until now the mass and volume of focusing X-ray optics have been too large for resource-limited in situ missions, so near-target X-ray observations of planetary bodies have been limited to simple collimator-type X-ray instruments. We introduce a new Miniature lightweight Wolter-I focusing X-ray Optics (MiXO) using metal-ceramic hybrid X-ray mirrors based on electroformed nickel replication and plasma thermal spray processes. MiXO can enable compact, powerful imaging X-ray telescopes suitable for future planetary missions. We illustrate the need for focusing X-ray optics in observing relatively small planetary bodies such as asteroids and comet nuclei. We present a few example configurations of MiXO telescopes and demonstrate their superior performance in comparison to an alternative approach, micro-pore optics, which is being employed for the first planetary focusing X-ray telescope, the Mercury Imaging X-ray Spectrometer-T onboard Bepicolumbo. X-ray imaging spectroscopy using MiXO will open a large new discovery space in planetary science and will greatly enhance our understanding of the nature and origin of diverse planetary bodies.
C1 [Hong, Jaesub] Harvard Univ, 60 Garden St, Cambridge, MA 02138 USA.
[Romaine, Suzanne] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
RP Hong, J (reprint author), Harvard Univ, 60 Garden St, Cambridge, MA 02138 USA.
EM jhong@cfa.harvard.edu
FU NASA [NNX12AG65G]
FX The travel expense for the symposium was supported by NASA Grant
NNX12AG65G. We thank Nicole D. Melso for performing simulations to
estimate the effective area and grasp for various telescope
configurations. We also thank Martin Elvis for the useful comments.
NR 18
TC 0
Z9 0
U1 3
U2 3
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD FEB 29
PY 2016
VL 68
BP 1
EP 8
AR 35
DI 10.1186/s40623-016-0409-1
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DE9DZ
UT WOS:000370937200001
ER
PT J
AU Martin-Drumel, MA
Roucou, A
Brown, GG
Thorwirth, S
Pirali, O
Mouret, G
Hindle, F
McCarthy, MC
Cuisset, A
AF Martin-Drumel, M. A.
Roucou, A.
Brown, G. G.
Thorwirth, S.
Pirali, O.
Mouret, G.
Hindle, F.
McCarthy, M. C.
Cuisset, A.
TI High resolution spectroscopy of six SOCl2 isotopologues from the
microwave to the far-infrared
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; QUADRUPOLE
COUPLING-CONSTANTS; THIONYL CHLORIDE; HYPERFINE-STRUCTURE; ROTATION
SPECTRUM; SULFURYL CHLORIDE; 2ND DERIVATIVES; MANY-BODY; GAS-PHASE
AB Despite its potential role as an atmospheric pollutant, thionyl chloride, SOCl2, remains poorly characterized in the gas phase. In this study, the pure rotational and ro-vibrational spectra of six isotopologues of this molecule, all detected in natural abundance, have been extensively studied from the cm-wave band to the far-infrared region by means of three complementary techniques: chirped-pulse Fourier transform microwave spectroscopy, sub-millimeter-wave spectroscopy using frequency multiplier chain, and synchrotron-based far-infrared spectroscopy. Owing to the complex line pattern which results from two nuclei with non-zero spins, new, high-level quantum-chemical calculations of the hyperfine structure played a crucial role in the spectroscopic analysis. From the combined experimental and theoretical work, an accurate semi-experimental equilibrium structure (r(e)(SE)) of SOCl2 has been derived. With the present data, spectroscopy-based methods can now be applied with confidence to detect and monitor this species, either by remote sensing or in situ. (C) 2016 AIP Publishing LLC.
C1 [Martin-Drumel, M. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Martin-Drumel, M. A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Roucou, A.; Mouret, G.; Hindle, F.; Cuisset, A.] Univ Littoral Cote dOpale, Lab Phys Chim Atmosphere, Dunkerque, France.
[Brown, G. G.] Coker Coll, Hartsville, SC 29550 USA.
[Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50931 Cologne, Germany.
[Pirali, O.] Synchrotron SOLEIL, AILES Beamline, St Aubin, France.
RP Martin-Drumel, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mmartin@cfa.harvard.edu
RI Hindle, Francis/B-3261-2009; Thorwirth, Sven/C-6217-2011;
OI Hindle, Francis/0000-0001-9925-4497; Thorwirth,
Sven/0000-0001-8200-6710; Martin-Drumel, Marie-Aline/0000-0002-5460-4294
FU French "Delegation Generale pour l'Armement" (Projet de Recherche
Exploratoire et Innovation) [06.34.037]; NASA [NNX13AE59G]; CfA
Postdoctoral Fellowship from Smithsonian Astrophysical Observatory; NSF
[1213560]; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-2]
FX The authors are grateful to SOLEIL for providing beamtime on the AILES
beamline under Proposal No. 20100693. We thank Dr. P. Roy and her team
(SOLEIL) and Dr. M. Guinet and Dr. S. Eliet (LPCA) for their help during
the experiments at SOLEIL. The submm work is supported by the French
"Delegation Generale pour l'Armement" (Projet de Recherche Exploratoire
et Innovation No. 06.34.037) and the CP-FTMW experimental work is
supported by NASA Grant No. NNX13AE59G. M.A.M.-D. is partially supported
by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical
Observatory. G.G.B. acknowledges the support of NSF Award No. 1213560.
S.T. gratefully acknowledges support by the Deutsche
Forschungsgemeinschaft (DFG) through Grant No. TH 1301/3-2. The authors
are thankful to Dr. M. Goubet for providing the Ph.D. thesis of J. L.
Journel.
NR 57
TC 1
Z9 1
U1 2
U2 16
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD FEB 28
PY 2016
VL 144
IS 8
AR 084305
DI 10.1063/1.4942024
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DF8OX
UT WOS:000371618800029
PM 26931700
ER
PT J
AU Malek, JC
Breitburg, DL
AF Malek, Jennafer C.
Breitburg, Denise L.
TI Effects of air-exposure gradients on spatial infection patterns of
Perkinsus marinus in the eastern oyster Crassostrea virginica
SO DISEASES OF AQUATIC ORGANISMS
LA English
DT Article
DE Intertidal exposure; Chesapeake Bay; Dermo disease; Perkinsiosis;
Estuary; Epizootic; Host-parasite system
ID CHESAPEAKE BAY; COMMUNITY STRUCTURE; ECOSYSTEM ENGINEERS; HABITAT
DEGRADATION; HEMOCYTES; PARASITE; DISEASE; REEFS; BIODIVERSITY;
TEMPERATURE
AB Spatial distributions of species can be shaped by factors such as parasites, mortality, and reproduction, all of which may be influenced by differences in physical factors along environmental gradients. In nearshore tidal waters, an elevational gradient in aerial exposure during low tide can shape the spatial distributions of benthic marine organisms. The eastern oyster Crassostrea virginica is an ecologically and economically important species that can dominate both subtidal and intertidal habitats along the east coast of the USA. Our goal was to determine whether prevalence and intensity of Perkinsus marinus (the causative agent of Dermo disease) infections vary along intertidal to subtidal gradients during summer. We used (1) field experiments conducted at 4 sites in the Chesapeake Bay and a Virginia coastal bay, (2) a controlled air-exposure experiment, and (3) field surveys from 7 sites ranging from Maine to North Carolina to test for effects of tidal exposure on infection. Results from our field surveys suggested that high intertidal oysters tend to have higher infection prevalence than subtidal oysters, but there was no effect on infection intensity. Field experiments rarely yielded significant effects of tidal exposure on infection prevalence and intensity. Overall, our study shows that exposure to air may not be a strong driver of infection patterns in this host-parasite system.
C1 [Malek, Jennafer C.; Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Malek, JC (reprint author), Univ Georgia, Georgia Sea Grant, 1180 E Broad St, Athens, GA 30602 USA.
EM malekjc1@uga.edu
FU MD Sea Grant; Smithsonian Endowments; Women's Committee; University of
Maryland
FX We thank MD Sea Grant, the Smithsonian Endowments, Graduate Fellowship
fund, and Women's Committee, and the University of Maryland for
providing funding for this research. We also thank Roger I. E. Newell
and Eric Schott for their contributions; all of the members of the
Marine Ecology Laboratory at the Smithsonian Environmental Research
Center from 2007 to 2010; Jennifer Jost and Kimberly Schneider for
assistance with mimic construction; Ryan Carnegie at VIMS for assistance
with parasite testing; and Ryan Carnegie and James Byers at UGA for
valuable comments and edits on earlier drafts of this manuscript.
NR 67
TC 1
Z9 1
U1 4
U2 7
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0177-5103
EI 1616-1580
J9 DIS AQUAT ORGAN
JI Dis. Aquat. Org.
PD FEB 25
PY 2016
VL 118
IS 2
BP 139
EP 151
DI 10.3354/dao02964
PG 13
WC Fisheries; Veterinary Sciences
SC Fisheries; Veterinary Sciences
GA DF4GP
UT WOS:000371306300004
PM 26912044
ER
PT J
AU Ambrosio, LJ
Baeza, JA
AF Ambrosio, Louis J.
Antonio Baeza, J.
TI Territoriality and Conflict Avoidance Explain Asociality (Solitariness)
of the Endosymbiotic Pea Crab Tunicotheres moseri
SO PLOS ONE
LA English
DT Article
ID PAGURUS-POLLICARIS SAY; IN-HOUSE CRICKETS; MATING SYSTEM; SEA-ANEMONE;
MARINE-INVERTEBRATES; HOST CHARACTERISTICS; LARVAL SETTLEMENT; CONVICT
CICHLIDS; BRACHYURAN CRABS; ANIMAL CONTESTS
AB Host monopolization theory predicts symbiotic organisms inhabiting morphologically simple, relatively small and scarce hosts to live solitarily as a result of territorial behaviors. We tested this prediction with Tunicotheres moseri, an endosymbiotic crab dwelling in the atrial chamber of the morphologically simple, small, and relatively scarce ascidian Styela plicata. As predicted, natural populations of T. moseri inhabit ascidian hosts solitarily with greater frequency than expected by chance alone. Furthermore, laboratory experiments demonstrated that intruder crabs take significantly longer to colonize previously infected compared to uninfected hosts, indicating as expected, that resident crabs exhibit monopolization behaviors. While territoriality does occur, agonistic behaviors employed by T. moseri do not mirror the overt behaviors commonly reported for other territorial crustaceans. Documented double and triple cohabitations in the field coupled with laboratory observations demonstrating the almost invariable success of intruder crabs colonizing occupied hosts, suggest that territoriality is ineffective in completely explaining the solitary social habit of this species. Additional experiments showed that T. moseri juveniles and adults, when searching for ascidians use chemical cues to avoid hosts occupied by conspecifics. This conspecific avoidance behavior reported herein is a novel strategy most likely employed to preemptively resolve costly territorial conflicts. In general, this study supports predictions central to host monopolization theory, but also implies that alternative behavioral strategies (i.e., conflict avoidance) may be more important than originally thought in explaining the host use pattern of symbiotic organisms.
C1 [Ambrosio, Louis J.; Antonio Baeza, J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
[Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA.
[Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo, Coquimbo, Chile.
RP Ambrosio, LJ (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
EM ljambro@g.clemson.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
NR 75
TC 2
Z9 2
U1 4
U2 9
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD FEB 24
PY 2016
VL 11
IS 2
AR e0148285
DI 10.1371/journal.pone.0148285
PG 20
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF2IA
UT WOS:000371164700007
PM 26910474
ER
PT J
AU Bayer, FM
van Ofwegen, LP
AF Bayer, F. M.
van Ofwegen, L. P.
TI The type specimens of Bebryce (Cnidaria, Octocorallia, Plexauridae)
re-examined, with emphasis on the sclerites
SO ZOOTAXA
LA English
DT Article
DE Bebryce; Discogorgia; re-descriptions; new species; SEM images; Siboga
AB Nineteen species of Bebryce are re-described and scanning electron microscopy (SEM) images of sclerites presented. For B. sulfurea Grasshoff, 2000, this is the first time SEM images of sclerites are presented. Two new species are described, Bebryce asteria n. sp. and B. cofferi n. sp., and B. stellata Hentschel, 1903 is synonymized with B. studeri Whitelegge, 1897. Bebryce acanthoides Thomson & Russell, 1910 is referred to Discogorgia Kukenthal, 1919. The status of the original type material is discussed.
C1 [Bayer, F. M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[van Ofwegen, L. P.] Naturalis Biodivers Ctr, POB 9517, NL-2300 RA Leiden, Netherlands.
RP Bayer, FM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM leen.vanofwegen@naturalis.nl; ofwegen@yahoo.com
NR 57
TC 1
Z9 1
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 22
PY 2016
VL 4083
IS 3
BP 301
EP 358
PG 58
WC Zoology
SC Zoology
GA DF6CD
UT WOS:000371441900001
PM 27394234
ER
PT J
AU Bernardi, G
Venturi, T
Cassano, R
Dallacasa, D
Brunetti, G
Cuciti, V
Johnston-Hollitt, M
Oozeer, N
Parekh, V
Smirnov, OM
AF Bernardi, G.
Venturi, T.
Cassano, R.
Dallacasa, D.
Brunetti, G.
Cuciti, V.
Johnston-Hollitt, M.
Oozeer, N.
Parekh, V.
Smirnov, O. M.
TI KAT-7 observations of an unbiased sample of mass-selected galaxy
clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium;
radio continuum: galaxies; radio continuum: general
ID DIFFUSE RADIO-EMISSION; SCALING RELATIONS; HALO SURVEY; MERGERS; MODEL;
SKY
AB The presence of megaparsec-scale radio haloes in galaxy clusters has already been established by many observations over the last two decades. The emerging explanation for the formation of these giant sources of diffuse synchrotron radio emission is that they trace turbulent regions in the intracluster medium, where particles are trapped and accelerated during cluster mergers. Our current observational knowledge is, however, mainly limited to massive systems. Here we present observations of a sample of 14 mass-selected galaxy clusters, i.e. M-500 > 4x10(14) M-circle dot, in the Southern hemisphere, aimed to study the occurrence of radio haloes in low-mass clusters and test the correlation between the radio halo power at 1.4 GHz P-1.4 and the cluster mass M-500. Our observations were performed with the 7-element Karoo Array Telescope at 1.86 GHz. We found three candidates to host diffuse cluster-scale emission and derived upper limits at the level of 0.6-1.9x10(24) Watt Hz(-1) for similar to 50 per cent of the clusters in the sample, significantly increasing the number of clusters with radio halo information in the considered mass range. Our results confirm that bright radio haloes in less massive galaxy clusters are statistically rare.
C1 [Bernardi, G.; Oozeer, N.; Smirnov, O. M.] SKA SA, 3rd Floor,Pk,Pk Rd, ZA-7405 Pinelands, South Africa.
[Bernardi, G.; Smirnov, O. M.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA.
[Venturi, T.; Cassano, R.; Brunetti, G.; Cuciti, V.] INAF, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
[Dallacasa, D.; Cuciti, V.] Univ Bologna, Dipartmento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Oozeer, N.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Muizenberg, South Africa.
[Oozeer, N.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Parekh, V.] Raman Res Inst, CV Raman Ave, Bengaluru 560080, Karnataka, India.
RP Bernardi, G (reprint author), SKA SA, 3rd Floor,Pk,Pk Rd, ZA-7405 Pinelands, South Africa.; Bernardi, G (reprint author), Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.; Bernardi, G (reprint author), Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA.; Venturi, T; Cassano, R (reprint author), INAF, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
EM gbernardi@ska.ac.za; tventuri@ira.inaf.it; rcassano@ira.inaf.it
FU National Research Foundation [92725]; Executive Programme of Scientific
and Technological Co-operation between the Italian Republic and the
Republic of South Africa; SKA South Africa; National Science Foundation
of South Africa; Ministry of Foreign Affairs and International
Cooperation, Directorate General for the Country Promotion [ZA14GR02]
FX We thank the referee for useful comments that helped improving the
manuscript. This work is based on research supported by the National
Research Foundation under grant 92725. Any opinion, finding and
conclusion or recommendation expressed in this material is that of the
author(s) and the NRF does not accept any liability in this regard. This
work was also partly supported by the Executive Programme of Scientific
and Technological Co-operation between the Italian Republic and the
Republic of South Africa 2014-2016. The KAT-7 is supported by SKA South
Africa and by the National Science Foundation of South Africa. With the
support of the Ministry of Foreign Affairs and International
Cooperation, Directorate General for the Country Promotion (Bilateral
Grant Agreement ZA14GR02 - Mapping the Universe on the Pathway to SKA).
NR 31
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 21
PY 2016
VL 456
IS 2
BP 1259
EP 1268
DI 10.1093/mnras/stv2589
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7KW
UT WOS:000372264200008
ER
PT J
AU Angus, R
Foreman-Mackey, D
Johnson, JA
AF Angus, Ruth
Foreman-Mackey, Daniel
Johnson, John A.
TI SYSTEMATICS-INSENSITIVE PERIODIC SIGNAL SEARCH WITH K2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE asteroseismology; methods: data analysis; methods: statistical; stars:
rotation; techniques: photometric
ID KEPLER LIGHT CURVES; STELLAR ROTATION; ERROR-CORRECTION; FIELD STARS;
MISSION; PHOTOMETRY; PLANETS; GYROCHRONOLOGY
AB From pulsating stars to transiting exoplanets, the search for periodic signals in K2 data, Kepler's two-wheeled extension, is relevant to a long list of scientific goals. Systematics affecting K2 light curves due to the decreased spacecraft pointing precision inhibit the easy extraction of periodic signals from the data. We here develop a method for producing periodograms of K2 light curves that are insensitive to pointing-induced systematics; the Systematics-insensitive Periodogram (SIP). Traditional sine-fitting periodograms use a generative model to find the frequency of a sinusoid that best describes the data. We extend this principle by including systematic trends, based on a set of "eigen light curves," following Foreman-Mackey et al., in our generative model as well as a sum of sine and cosine functions over a grid of frequencies. Using this method we are able to produce periodograms with vastly reduced systematic features. The quality of the resulting periodograms are such that we can recover acoustic oscillations in giant stars and measure stellar rotation periods without the need for any detrending. The algorithm is also applicable to the detection of other periodic phenomena such as variable stars, eclipsing binaries and short-period exoplanet candidates. The SIP code is available at https://github.com/RuthAngus/SIPK2.
C1 [Angus, Ruth] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Angus, Ruth; Johnson, John A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Foreman-Mackey, Daniel] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
RP Angus, R (reprint author), Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.; Angus, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ruthangus@gmail.com
FU David and Lucile Packard Foundation; Alfred P. Sloan Foundation; NASA
[NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA Science
Mission directorate
FX It is a pleasure to thank Dan Huber (Sydney) who provided many excellent
comments for this paper and useful asteroseismology tips. We would also
like to thank David Hogg (NYU) and Suzanne Aigrain (Oxford) for their
comments, plus Andrew Vanderburg (Harvard), Ben Montet (Caltech) and
Stephanie Douglas (Columbia) for their extremely helpful suggestions and
recommendations regarding this project. J.A.J. is supported by generous
grants from the David and Lucile Packard and Alfred P. Sloan
Foundations. The data presented in this paper were obtained from the
Mikulski Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts. This paper includes data collected by the Kepler
mission. Funding for the Kepler mission is provided by the NASA Science
Mission directorate.
NR 25
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 109
DI 10.3847/0004-637X/818/2/109
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800008
ER
PT J
AU Bai, XN
Ye, JN
Goodman, J
Yuan, F
AF Bai, Xue-Ning
Ye, Jiani
Goodman, Jeremy
Yuan, Feng
TI MAGNETO-THERMAL DISK WINDS FROM PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; magnetohydrodynamics (MHD); methods:
numerical; protoplanetary disks
ID YOUNG STELLAR OBJECTS; MAGNETICALLY-DRIVEN JETS; ACCRETION-EJECTION
STRUCTURES; T-TAURI STARS; WEAKLY MAGNETIZED DISKS; ACTIVE GALACTIC
NUCLEI; X-RAY IONIZATION; MAGNETOROTATIONAL-INSTABILITY; CIRCUMSTELLAR
DISKS; PLANETESIMAL FORMATION
AB The global evolution and dispersal of protoplanetary disks (PPDs) are governed by disk angular-momentum transport and mass-loss processes. Recent numerical studies suggest that angular-momentum transport in the inner region of PPDs is largely driven by magnetized disk wind, yet the wind mass-loss rate remains unconstrained. On the other hand, disk mass loss has conventionally been attributed to photoevaporation, where external heating on the disk surface drives a thermal wind. We unify the two scenarios by developing a one-dimensional model of magnetized disk winds with a simple treatment of thermodynamics as a proxy for external heating. The wind properties largely depend on (1) the magnetic field strength at the wind base, characterized by the poloidal Alfven speed nu(Ap), (2) the sound speed c(s) near the wind base, and (3) how rapidly poloidal field lines diverge (achieve R-2 scaling). When nu(Ap) >> c(s), corotation is enforced near the wind base, resulting in centrifugal acceleration. Otherwise, the wind is accelerated mainly by the pressure of the toroidal magnetic field. In both cases, the dominant role played by magnetic forces likely yields wind outflow rates that exceed purely hydrodynamical mechanisms. For typical PPD accretion-rate and wind-launching conditions, we expect nu(Ap) to be comparable to c(s) at the wind base. The resulting wind is heavily loaded, with a total wind mass-loss rate likely reaching a considerable fraction of the wind-driven accretion rate. Implications for modeling global disk evolution and planet formation are also discussed.
C1 [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
[Ye, Jiani; Yuan, Feng] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China.
[Goodman, Jeremy] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM xbai@cfa.harvard.edu
FU Institute for Theory and Computation (ITC) at Harvard-Smithsonian Center
for Astrophysics; NASA [NNX10AH37G]; NSF of China [11133005, 11573051];
CAS [XDB09000000]
FX We thank the Institute for Advanced Study at Tsinghua University
(IASTU), Beijing, for hosting the spring school on planet formation in
May 2014, where this project was initiated, and thank Doug Lin and Dong
Lai for their initiatives in organizing the spring school. We have
benefited from Uma Gorti, Geoffroy Lesur, and Eve Ostriker for useful
discussions, and an anonymous referee report. X.N.B. acknowledges
support from Institute for Theory and Computation (ITC) at
Harvard-Smithsonian Center for Astrophysics. J.G. acknowledges support
from the NASA Origins of Solar Systems program via grant NNX10AH37G.
F.Y. acknowledges support by the NSF of China (grants 11133005 and
11573051), and the Strategic Priority Research Program The Emergence of
Cosmological Structures of CAS (grant XDB09000000).
NR 166
TC 1
Z9 1
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 152
DI 10.3847/0004-637X/818/2/152
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800051
ER
PT J
AU Basu-Zych, AR
Lehmer, B
Fragos, T
Hornschemeier, A
Yukita, M
Zezas, A
Ptak, A
AF Basu-Zych, Antara R.
Lehmer, Bret
Fragos, Tassos
Hornschemeier, Ann
Yukita, Mihoko
Zezas, Andreas
Ptak, Andy
TI EXPLORING THE OVERABUNDANCE OF ULXs IN METAL- AND DUST-POOR LOCAL LYMAN
BREAK ANALOGS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: individual (Haro 11, VV 114); galaxies:
starburst; X-rays: binaries; X-rays: galaxies
ID X-RAY SOURCES; STAR-FORMATION RATE; MASS-METALLICITY RELATION; CHANDRA
MONITORING OBSERVATIONS; ULTRAVIOLET-LUMINOUS GALAXIES; NEARBY STARBURST
GALAXIES; COMPACT OBJECT FORMATION; UV-SELECTED GALAXIES; BLACK-HOLE
BINARIES; MERGER VV 114
AB We have studied high-mass X-ray binary (HMXB) populations within two low-metallicity, starburst galaxies, Haro 11 and VV 114. These galaxies serve as analogs to high-redshift (z > 2) Lyman break galaxies and, within the larger sample of Lyman break analogs (LBAs), they are sufficiently nearby (<87 Mpc) to be spatially resolved by Chandra. Previous studies of the X-ray emission in LBAs have found that the 2-10 keV. luminosity per star formation rate (SFR) in these galaxies is elevated, potentially because of their low metallicities (12 + log[O/H] = 8.3-8.4). Theoretically, the progenitors of XRBs forming in lower metallicity environments lose less mass from stellar winds over their lifetimes, producing more massive compact objects (i.e.,. neutron stars and black holes), and thus resulting in more numerous and luminous HMXBs per SFR. In this paper, we have performed an in-depth study of the only two LBAs that have spatially resolved 2-10 keV. emission with Chandra. to present the bright end of the X-ray luminosity distribution of HMXBs (L-X greater than or similar to 10(39) erg s(-1); ultraluminous X-ray sources, ULXs) in these low-metallicity galaxies, based on eight detected ULXs. Compared with the star-forming galaxy X-ray luminosity function (XLF) presented by Mineo et al., Haro 11 and VV 114 host approximate to 4 times more L-X > 10(40) erg s(-1). sources than expected given their SFRs. We simulate the effects of source blending from crowded lower-luminosity HMXBs using the star-forming galaxy XLF and then vary the XLF normalizations and bright-end slopes until we reproduce the observed point source luminosity distributions. We find that these LBAs have a shallower bright-end slope (gamma(2) = 1.90) than the standard XLF (gamma(2) = 2.73). If we conservatively assume that the brightest X-ray source from each galaxy is powered by an accreting supermassive black hole rather than an HMXB and eliminate these sources from consideration, the luminosity distribution becomes poorly constrained but does appear to be consistent with a standard XLF.
C1 [Basu-Zych, Antara R.; Lehmer, Bret; Hornschemeier, Ann; Yukita, Mihoko; Ptak, Andy] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Basu-Zych, Antara R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Lehmer, Bret] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA.
[Lehmer, Bret] Univ Arkansas, Dept Phys, 825 West Dickson St, Fayetteville, AR 72701 USA.
[Fragos, Tassos] Univ Geneva, Observ Geneva, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland.
[Yukita, Mihoko] Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
[Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Zezas, Andreas] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Zezas, Andreas] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece.
[Zezas, Andreas] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece.
RP Basu-Zych, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.; Basu-Zych, AR (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RI Yukita, Mihoko/E-4135-2017; Zezas, Andreas/C-7543-2011; Fragos,
Tassos/A-3581-2016
OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523
FU NASA Astrophysics Data Analysis Program (ADAP) [09-ADP09-0071]; Swiss
National Science Foundation [PZ00P2_148123]; European Research Council
under the European Union/ERC [617001]; NASA/ADAP [NNX12AN05G]
FX We thank the referee for helpful suggestions that improved the
manuscript. A.R.B. and A.H. gratefully acknowledge the NASA Astrophysics
Data Analysis Program (ADAP grant 09-ADP09-0071, PI: A. Hornschemeier)
for providing financial support. T.F. acknowledges support from the
Ambizione Fellowship of the Swiss National Science Foundation (grant
PZ00P2_148123). A.Z. acknowledges funding from the European Research
Council under the European Union's Seventh Framework Programme
(FP/2007-2013)/ERC Grant Agreement n. 617001 and financial support from
NASA/ADAP grant NNX12AN05G.
NR 97
TC 0
Z9 0
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 140
DI 10.3847/0004-637X/818/2/140
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800039
ER
PT J
AU Bovy, J
Rix, HW
Green, GM
Schlafly, EF
Finkbeiner, DP
AF Bovy, Jo
Rix, Hans-Walter
Green, Gregory M.
Schlafly, Edward F.
Finkbeiner, Douglas P.
TI ON GALACTIC DENSITY MODELING IN THE PRESENCE OF DUST EXTINCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; Galaxy: kinematics and dynamics; Galaxy: structure;
methods: data analysis; stars: statistics; surveys
ID MILKY-WAY DISK; APOGEE; PHOTOMETRY; MAP
AB Inferences about the spatial density or phase-space structure of stellar populations in the Milky Way require a precise determination of the effective survey volume. The volume observed by surveys such as Gaia or near-infrared spectroscopic surveys, which have good coverage of the Galactic midplane region, is highly complex because of the abundant small-scale structure in the three-dimensional interstellar dust extinction. We introduce a novel framework for analyzing the importance of small-scale structure in the extinction. This formalism demonstrates that the spatially complex effect of extinction on the selection function of a pencil-beam or contiguous sky survey is equivalent to a low-pass filtering of the extinction-affected selection function with the smooth density field. We find that the angular resolution of current 3D extinction maps is sufficient for analyzing Gaia sub-samples of millions of stars. However, the current distance resolution is inadequate and needs to be improved by an order of magnitude, especially in the inner Galaxy. We also present a practical and efficient method for properly taking the effect of extinction into account in analyses of Galactic structure through an effective selection function. We illustrate its use with the selection function of red-clump stars in APOGEE using and comparing a variety of current 3D extinction maps.
C1 [Bovy, Jo] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Bovy, Jo] Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA.
[Rix, Hans-Walter; Schlafly, Edward F.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Green, Gregory M.; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Bovy, J (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.; Bovy, J (reprint author), Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA.
EM bovy@astro.utoronto.ca
OI Green, Gregory/0000-0001-5417-2260
FU John N. Bahcall Fellowship; W. M. Keck Foundation; Natural Sciences and
Engineering Research Council of Canada; European Research Council under
the European Union ERC [321035]; Kavli Institute for Theoretical Physics
in Santa Barbara
FX It is a pleasure to thank the anonymous referee and Wilma Trick for
helpful comments. Some of the results in this paper have been derived
using the HEALPix (Gorski et al. 2005) and healpy packages. J.B.
received support from a John N. Bahcall Fellowship, the W. M. Keck
Foundation, and the Natural Sciences and Engineering Research Council of
Canada. H.W.R. received funding for this research from the European
Research Council under the European Union's Seventh Framework Programme
(FP 7) ERC Grant Agreement no. [321035]. J.B. and H.W.R. acknowledge the
generous support and hospitality of the Kavli Institute for Theoretical
Physics in Santa Barbara during the "Galactic Archaeology and Precision
Stellar Astrophysics" program, where some of this research was
performed.
NR 15
TC 4
Z9 4
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 130
DI 10.3847/0004-637X/818/2/130
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800029
ER
PT J
AU Brown, WR
Gianninas, A
Kilic, M
Kenyon, SJ
Prieto, CA
AF Brown, Warren R.
Gianninas, A.
Kilic, Mukremin
Kenyon, Scott J.
Allende Prieto, Carlos
TI THE ELM SURVEY. VII. ORBITAL PROPERTIES OF LOW-MASS WHITE DWARF BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; Galaxy: stellar content; white dwarfs
ID COMMON ENVELOPE BINARIES; 3D MODEL ATMOSPHERES; R-CORONAE-BOREALIS; AM
CVN STARS; M-CIRCLE-DOT; DOUBLE-DEGENERATE; GRAVITATIONAL-WAVES;
SPECTROSCOPIC ANALYSIS; RADIAL-VELOCITIES; MERGER SYSTEMS
AB We present the discovery of 15 extremely low-mass (5 < log g < 7) white dwarf (WD) candidates, 9 of which are in ultra-compact double-degenerate binaries. Our targeted extremely low-mass Survey sample now includes 76 binaries. The sample has a lognormal distribution of orbital periods with a median period of 5.4 hr. The velocity amplitudes imply that the binary companions have a normal distribution of mass with 0.76 M-circle dot mean and 0.25 M-circle dot dispersion. Thus extremely low-mass WDs are found in binaries with a typical mass ratio of 1:4. Statistically speaking, 95% of the WD binaries have a total mass below the Chandrasekhar mass, and thus are not type Ia supernova progenitors. Yet half of the observed binaries will merge in less than 6 Gyr due to gravitational wave radiation; probable outcomes include single massive WDs and stable mass transfer AM CVn binaries.
C1 [Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Gianninas, A.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
RP Brown, WR; Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Gianninas, A; Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.; Prieto, CA (reprint author), Inst Astrofis Canarias, E-38205 Tenerife, Spain.; Prieto, CA (reprint author), Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
EM wbrown@cfa.harvard.edu; alexg@nhn.ou.edu; kilic@ou.edu;
skenyon@cfa.harvard.edu; callende@iac.es
RI Alexandros, Gianninas/B-8352-2016
OI Alexandros, Gianninas/0000-0002-8655-4308
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England; Smithsonian Institution; NSF; NASA [AST-1312678, NNX14AF65G]
FX We thank Charlotte Wood for her contribution to the spectral energy
distributions. We thank E. Martin, A. Milone, and S. Gotilla for their
assistance with observations obtained at the MMT Observatory, P. Canton
for his assistance with observations obtained at Kitt Peak National
Observatory, and P. Berlind and M. Calkins for their assistance with
observations obtained at the Fred Lawrence Whipple Observatory. This
project makes use of data products from SDSS and SDSS-II, funding for
which was provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the U.S. Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. This research makes use the SAO/NASA Astrophysics
Data System Bibliographic Service. This work was supported in part by
the Smithsonian Institution. M.K. and A.G. gratefully acknowledge the
support of the NSF and NASA under grants AST-1312678 and NNX14AF65G,
respectively.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
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DI 10.3847/0004-637X/818/2/155
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800054
ER
PT J
AU Bulbul, E
Randall, SW
Bayliss, M
Miller, E
Andrade-Santos, F
Johnson, R
Bautz, M
Blanton, EL
Forman, WR
Jones, C
Paterno-Mahler, R
Murray, SS
Sarazin, CL
Smith, RK
Ezer, C
AF Bulbul, Esra
Randall, Scott W.
Bayliss, Matthew
Miller, Eric
Andrade-Santos, Felipe
Johnson, Ryan
Bautz, Mark
Blanton, Elizabeth L.
Forman, William R.
Jones, Christine
Paterno-Mahler, Rachel
Murray, Stephen S.
Sarazin, Craig L.
Smith, Randall K.
Ezer, Cemile
TI PROBING THE OUTSKIRTS OF THE EARLY-STAGE GALAXY CLUSTER MERGER A1750
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (A1750); large-scale structure of
universe; X-rays: galaxies: clusters
ID X-RAY SPECTROSCOPY; DARK-MATTER HALOS; VIRIAL RADIUS; REPRESENTATIVE
SAMPLE; PHYSICAL-PROPERTIES; INTRACLUSTER MEDIUM; SUZAKU OBSERVATIONS;
CENTAURUS CLUSTER; ANALYTIC MODEL; GAS PROPERTIES
AB We present results from recent Suzaku and Chandra X-ray and Multiple Mirrior Telescope optical observations of the strongly merging "double cluster" A1750 out to its virial radius, both along and perpendicular to a putative large-scale structure filament. Some previous studies of individual clusters have found evidence for ICM entropy profiles that flatten at large cluster radii, as compared with the self-similar prediction based on purely gravitational models of hierarchical cluster formation, and gas fractions that rise above the mean cosmic value. Weakening accretion shocks and the presence of unresolved cool gas clumps, both of which are expected to correlate with large-scale structure filaments, have been invoked to explain these results. In the outskirts of A1750, we find entropy profiles that are consistent with self-similar expectations, and gas fractions that are consistent with the mean cosmic value, both along and perpendicular to the putative large-scale filament. Thus, we find no evidence for gas clumping in the outskirts of A1750, in either direction. This may indicate that gas clumping is less common in lower temperature (kT approximate to 4 keV), less massive systems, consistent with some (but not all) previous studies of low-mass clusters and groups. Cluster mass may, therefore, play a more important role in gas clumping than dynamical state. Finally, we find evidence for diffuse, cool (<1 keV) gas at large cluster radii (R-200) along the filament, which is consistent with the expected properties of the denser, hotter phase of the warm-hot intergalactic medium.
C1 [Bulbul, Esra; Randall, Scott W.; Bayliss, Matthew; Andrade-Santos, Felipe; Forman, William R.; Jones, Christine; Murray, Stephen S.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bayliss, Matthew] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
[Miller, Eric; Bautz, Mark] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Johnson, Ryan] Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA.
[Blanton, Elizabeth L.; Paterno-Mahler, Rachel] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Blanton, Elizabeth L.; Paterno-Mahler, Rachel] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Paterno-Mahler, Rachel] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Sarazin, Craig L.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[Ezer, Cemile] Bogazici Univ, Dept Phys, Istanbul, Turkey.
RP Bulbul, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [NNX13AE83G, NNX10AR29G]; Chandra X-ray Center through NASA
[NAS8-03060]; Smithsonian Institution; NSF [AST-1009012]; National
Science Foundation [AST-1309032]; Chandra grants [GO4-15123X,
GO5-16131X, GO2-13152X, GO3-14132X]; NASA XMM [NNX15AG26G]
FX We thank Gabriel Pratt for kindly providing temperature, density, and
entropy profiles from XMM-Newton data. We also thank Mike McDonald and
John Zuhone for useful comments and suggestions. E.B. was supported in
part by NASA grants NNX13AE83G and NNX10AR29G. S.W.R. was supported by
the Chandra X-ray Center through NASA contract NAS8-03060 and by the
Smithsonian Institution. M.B.B. acknowledges support from the NSF
through grant AST-1009012. E.L.B. and R.P.M. was partially supported by
the National Science Foundation through grant AST-1309032. C.L.S. was
funded in part by Chandra grants GO4-15123X and GO5-16131X and NASA XMM
grant NNX15AG26G. A.E.D.M. acknowledges partial support by Chandra
grants GO2-13152X and GO3-14132X. The authors thank Prof. Dr. Nihal E.
Ercan for providing the support for C.E.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800030
ER
PT J
AU Burns, E
Connaughton, V
Zhang, BB
Lien, A
Briggs, MS
Goldstein, A
Pelassa, V
Troja, E
AF Burns, Eric
Connaughton, Valerie
Zhang, Bin-Bin
Lien, Amy
Briggs, Michael S.
Goldstein, Adam
Pelassa, Veronique
Troja, Eleonora
TI DO THE FERMI GAMMA-RAY BURST MONITOR AND SWIFT BURST ALERT TELESCOPE SEE
THE SAME SHORT GAMMA-RAY BURSTS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general
ID MERGING NEUTRON-STARS; LONG; MERGERS; GRB; CLASSIFICATION; ERA
AB Compact binary system mergers are expected to generate gravitational radiation detectable by ground-based interferometers. A subset of these, the merger of a neutron star with another neutron star or a black hole, are also the most popular model for the production of short gamma-ray bursts (GRBs). The Swift Burst Alert Telescope (BAT) and the Fermi Gamma-ray Burst Monitor (GBM) trigger on short GRBs (SGRBs) at rates that reflect their relative sky exposures, with the BAT detecting 10 per year compared to about 45 for GBM. We examine the SGRB populations detected by Swift BAT and Fermi GBM. We find that the Swift BAT triggers on weaker SGRBs than Fermi GBM, providing they occur close to the center of the BAT field of view, and that the Fermi GBM SGRB detection threshold remains flatter across its field of view. Overall, these effects combine to give the instruments the same average sensitivity, and account for the SGRBs that trigger one instrument but not the other. We do not find any evidence that the BAT and GBM are detecting significantly different populations of SGRBs. Both instruments can detect untriggered SGRBs using ground searches seeded with time and position. The detection of SGRBs below the on-board triggering sensitivities of Swift BAT and Fermi GBM increases the possibility of detecting and localizing the electromagnetic counterparts of gravitational wave (GW) events seen by the new generation of GW detectors.
C1 [Burns, Eric; Briggs, Michael S.] Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Connaughton, Valerie] Univ Space Res Assoc, Inst Sci & Technol, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Zhang, Bin-Bin] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Lien, Amy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goldstein, Adam] NASA, Postdoctoral Program, Space Sci Off, Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA.
[Pelassa, Veronique] Smithsonian Astrophys Observ, POB 97, Amado, AZ 85645 USA.
[Troja, Eleonora] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Burns, E (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM eb0016@uah.edu
FU GBM [NNM11AA01A/MSFC]; NASA Swift GI grant [NNX15AC05G]
FX We would like to acknowledge the contributions of two people. David
Palmer who generated BAT lightcurves, allowing us to further investigate
GBM SGRBs as viewed by the BAT, and Hans Krimm who compiled continuous
attitude files for Swift, saving us a great deal of time. We
additionally recognize the efforts of the HEASARC in providing the
searchable databases that were the source of our data. The GBM members
acknowledge support from GBM through NNM11AA01A/MSFC. Eric Burns
acknowledges support through NASA Swift GI grant NNX15AC05G.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
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PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800009
ER
PT J
AU Correia, C
Lazarian, A
Burkhart, B
Pogosyan, D
De Medeiros, JR
AF Correia, C.
Lazarian, A.
Burkhart, B.
Pogosyan, D.
De Medeiros, J. R.
TI PRINCIPAL COMPONENT ANALYSIS STUDIES OF TURBULENCE IN OPTICALLY THICK
GAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: structure; magnetohydrodynamics (MHD); methods: numerical
ID VELOCITY-FIELD STATISTICS; INTERSTELLAR TURBULENCE; MOLECULAR CLOUDS;
MAGNETOHYDRODYNAMIC TURBULENCE; POWER SPECTRUM; STAR-FORMATION; DENSITY;
ANISOTROPY; RETRIEVAL
AB In this work we investigate the sensitivity of principal component analysis (PCA) to the velocity power spectrum in high-opacity regimes of the interstellar medium (ISM). For our analysis we use synthetic position-position-velocity (PPV) cubes of fractional Brownian motion and magnetohydrodynamics (MHD) simulations, post-processed to include radiative transfer effects from CO. We find that PCA analysis is very different from the tools based on the traditional power spectrum of PPV data cubes. Our major finding is that PCA is also sensitive to the phase information of PPV cubes and this allows PCA to detect the changes of the underlying velocity and density spectra at high opacities, where the spectral analysis of the maps provides the universal -3 spectrum in accordance with the predictions of the Lazarian & Pogosyan theory. This makes PCA a potentially valuable tool for studies of turbulence at high opacities, provided that proper gauging of the PCA index is made. However, we found the latter to not be easy, as the PCA results change in an irregular way for data with high sonic Mach numbers. This is in contrast to synthetic Brownian noise data used for velocity and density fields that show monotonic PCA behavior. We attribute this difference to the PCA's sensitivity to Fourier phase information.
C1 [Correia, C.; De Medeiros, J. R.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil.
[Lazarian, A.] Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53711 USA.
[Burkhart, B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA.
[Pogosyan, D.] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 1A1, Canada.
RP Correia, C (reprint author), Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil.
EM caioftc@dfte.ufrn.br
FU CNPq; FAPERN; INCT-INEspaco; PDJ/CAPES [88887.114342/2015-00]; NASA
FX The research activities of the Observational Astronomy Stellar Board at
the Federal University of Rio Grande do Norte are supported by
continuous grants from the Brazilian agencies CNPq and FAPERN and by the
INCT-INEspaco. C.C. acknowledges a PDJ/CAPES fellowship (Process no
88887.114342/2015-00). B.B. acknowledges the support of the NASA
Einstein Postdoctoral Fellowship. A.L. acknowledges the support from the
Center for Magnetic Self-Organization, a distinguished visitor PVE/CAPES
appointment at the Physics Graduate Program at UFRN, Natal, Brazil and
thanks the DFTE/UFRN for hospitality.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
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PG 9
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SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800017
ER
PT J
AU Czekala, I
Andrews, SM
Torres, G
Jensen, ELN
Stassun, KG
Wilner, DJ
Latham, DW
AF Czekala, I.
Andrews, S. M.
Torres, G.
Jensen, E. L. N.
Stassun, K. G.
Wilner, D. J.
Latham, D. W.
TI A DISK-BASED DYNAMICAL CONSTRAINT ON THE MASS OF THE YOUNG BINARY DQ TAU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE protoplanetary disks; stars: fundamental parameters; stars: individual
(DQ Tau); stars: pre-main sequence
ID MAIN-SEQUENCE TRACKS; T-TAURI; STARS. I.; CIRCUMSTELLAR DISKS;
RADIAL-VELOCITIES; EVOLUTION; SYSTEM; ISOCHRONES; ACCRETION; DATABASE
AB We present new Atacama Large Millimeter/Submillimeter Array (ALMA) observations of CO J = 2-1 line emission from the DQ. Tau circumbinary disk. These data are used to tomographically reconstruct the Keplerian disk velocity field in a forward-modeling inference framework, and thereby provide a dynamical constraint on the mass of the DQ. Tau binary of M-* = 1.27(-0.27)(+0.46)M(circle dot). Those results are compared with an updated and improved orbital solution for this double-lined system based on long-term monitoring of its stellar radial velocities. Both of these independent dynamical constraints on the binary mass are in excellent agreement: taken together, they demonstrate that the DQ. Tau system mass is 1.21 +/- 0.26 M-circle dot and that the disk and binary orbital planes are aligned within 3 degrees (at 3 sigma confidence). The predictions of various theoretical models for pre-main-sequence stellar evolution are also consistent with these masses, though more detailed comparisons are difficult due to lingering uncertainties regarding the photospheric properties of the individual components. DQ. Tau is the third, nearly equal-mass, double-lined spectroscopic binary with a circumbinary disk that has been dynamically "weighed" with these two independent techniques: all show consistent results, validating the overall accuracy of the disk-based approach and demonstrating that it can be robustly applied to large samples of young, single stars as ALMA ramps up to operations at full capacity.
C1 [Czekala, I.; Andrews, S. M.; Torres, G.; Wilner, D. J.; Latham, D. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Jensen, E. L. N.] Swarthmore Coll, Dept Phys & Astron, 500 Coll Ave, Swarthmore, PA 19081 USA.
[Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
RP Czekala, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM iczekala@cfa.harvard.edu
OI Jensen, Eric/0000-0002-4625-7333; Czekala, Ian/0000-0002-1483-8811
FU Smithsonian Institution
FX We appreciate some useful computational suggestions from Ryan Loomis.
I.C. gratefully acknowledges funding support from the Smithsonian
Institution. S.A. appreciates the very helpful support provided by the
NRAO Student Observing Support program related to the early development
of this project. This paper makes use of the following ALMA data:
2012.1.00496.S. ALMA is a partnership of ESO (representing its member
states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC
and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint
ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. Figure 2 was
generated with the triangle.py code (Foreman-Mackey et al. 2014). This
research made extensive use of the Julia programming language (Bezanson
et al. 2012) and Astropy software package (Astropy Collaboration 2013).
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
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ER
PT J
AU Dittmann, JA
Irwin, JM
Charbonneau, D
Newton, ER
AF Dittmann, Jason A.
Irwin, Jonathan M.
Charbonneau, David
Newton, Elisabeth R.
TI CALIBRATION OF THE MEARTH PHOTOMETRIC SYSTEM: OPTICAL MAGNITUDES AND
PHOTOMETRIC METALLICITY ESTIMATES FOR 1802 NEARBY M-DWARFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; solar neighborhood; stars: abundances; stars: fundamental
parameters; stars: low-mass; techniques: photometric
ID PROPER-MOTION STARS; ALL-SKY SURVEY; LOW-MASS STARS; PROGRAM
TRIGONOMETRIC PARALLAXES; CANDIDATE HOST STARS; LSPM-NORTH CATALOG;
GUIDANCE SENSOR 3; K-BAND SPECTRA; SOLAR NEIGHBORHOOD; COOL NEIGHBORS
AB The MEarth Project is a photometric survey systematically searching the smallest stars near the Sun for transiting rocky planets. Since 2008, MEarth has taken approximately two million images of 1844 stars suspected to be mid-to-late M dwarfs. We have augmented this survey by taking nightly exposures of photometric standard stars and have utilized this data to photometrically calibrate the MEarth system, identify photometric nights, and obtain an optical magnitude with 1.5% precision for each M dwarf system. Each optical magnitude is an average over many years of data, and therefore should be largely immune to stellar variability and flaring. We combine this with trigonometric distance measurements, spectroscopic metallicity measurements, and 2MASS infrared magnitude measurements in order to derive a color-magnitude-metallicity relation across the mid-to-late M dwarf spectral sequence that can reproduce spectroscopic metallicity determinations to a precision of 0.1 dex. We release optical magnitudes and metallicity estimates for 1567 M dwarfs, many of which did not have an accurate determination of either prior to this work. For an additional 277 stars without a trigonometric parallax, we provide an estimate of the distance, assuming solar neighborhood metallicity. We find that the median metallicity for a volume-limited sample of stars within 20 pc of the Sun is [Fe/H] = -0.03 +/- 0.008, and that 29/565 of these stars have a metallicity of [Fe/H] = -0.5 or lower, similar to the low-metallicity distribution of nearby G dwarfs. When combined with the results of ongoing and future planet surveys targeting these objects, the metallicity estimates presented here will be important for assessing the significance of any putative planet-metallicity correlation.
C1 [Dittmann, Jason A.; Irwin, Jonathan M.; Charbonneau, David; Newton, Elisabeth R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Dittmann, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU National Science Foundation; University of Texas at Austin; David and
Lucille Packard Fellowship for Science and Engineering; National Science
Foundation [AST-0807690, AST-1109468, AST-1004488]; John Templeton
Foundation; NASA; NSF
FX We thank the anonymous referee for insight and suggestions during the
review of this manuscript. E.R.N. was supported throughout this work by
a National Science Foundation Graduate Research Fellowship and A.W.M. by
the Harlan J. Smith Fellowship from the University of Texas at Austin.
The MEarth Team gratefully acknowledges funding from the David and
Lucille Packard Fellowship for Science and Engineering (awarded to
D.C.). This material is based upon work supported by the National
Science Foundation under grants AST-0807690, AST-1109468, and
AST-1004488 (Alan T. Waterman Award). This publication was made possible
through the support of a grant from the John Templeton Foundation. The
opinions expressed in this publication are those of the authors and do
not necessarily reflect the views of the John Templeton Foundation. This
research has made extensive use of data products from the Two Micron All
Sky Survey, which is a joint project of the University of Massachusetts
and the Infrared Processing and Analysis Center/California Institute of
Technology, funded by NASA and the NSF, NASA's Astrophysics Data System
(ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. The
MEarth team would also like to acknowledge Eric Mamajek, who initially
suggested that we engage in this work. The authors of this paper would
also like to thank Zachory Berta-Thompson, whose comments, suggestions,
and extensive work with the MEarth observatory and data are invaluable.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800052
ER
PT J
AU Gomez, DO
DeLuca, EE
Mininni, PD
AF Gomez, Daniel O.
DeLuca, Edward E.
Mininni, Pablo D.
TI SIMULATIONS OF THE KELVIN-HELMHOLTZ INSTABILITY DRIVEN BY CORONAL MASS
EJECTIONS IN THE TURBULENT CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; magnetohydrodynamics; Sun: coronal mass ejections;
turbulence
ID SHEAR-FLOW; MAGNETOSPHERIC BOUNDARY; COMPRESSIBLE PLASMA;
MAGNETIC-FIELDS; SOLAR CORONA; STABILITY; MHD; DYNAMICS; LAYER;
RECONNECTION
AB Recent high-resolution Atmospheric Imaging Assembly/Solar Dynamics Observatory. images show evidence of the development of the Kelvin-Helmholtz (KH) instability, as coronal mass ejections (CMEs) expand in the ambient corona. A large-scale magnetic field mostly tangential to the interface is inferred, both on the CME and on the background sides. However, the magnetic field component along the shear flow is not strong enough to quench the instability. There is also observational evidence that the ambient corona is in a turbulent regime, and therefore the criteria for the development of the instability are a priori expected to differ from the laminar case. To study the evolution of the KH instability with a turbulent background, we perform three-dimensional simulations of the incompressible magnetohydrodynamic equations. The instability is driven by a velocity profile tangential to the CME-corona interface, which we simulate through a hyperbolic tangent profile. The turbulent background is generated by the application of a stationary stirring force. We compute the instability growth rate for different values of the turbulence intensity, and find that the role of turbulence is to attenuate the growth. The fact that KH instability is observed sets an upper limit on the correlation length of the coronal background turbulence.
C1 [Gomez, Daniel O.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Mininni, Pablo D.] Univ Buenos Aires, Dept Fis, Fac Ciencias Exactas & Nat, Ciudad Univ, RA-1428 Buenos Aires, DF, Argentina.
[Mininni, Pablo D.] Inst Fis Buenos Aires, Ciudad Univ, RA-1428 Buenos Aires, DF, Argentina.
RP Gomez, DO (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C]; PICT from ANPCyT
[0454/2011]; PICTs from ANPCyT (Argentina) [2011-1529, 2011-1626]
FX D.G. and E.E.D. acknowledge financial support from grant SP02H1701R from
Lockheed-Martin to SAO. E.E.D. was also supported by NASA contract
NNM07AB07C. D.G. also acknowledges support from PICT grant 0454/2011
from ANPCyT to IAFE and P.D.M. acknowledges support from PICTs 2011-1529
and 2011-1626 from ANPCyT to IFIBA (Argentina).
NR 42
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
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AR 126
DI 10.3847/0004-637X/818/2/126
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800025
ER
PT J
AU Hwang, HS
Geller, MJ
Park, C
Fabricant, DG
Kurtz, MJ
Rines, KJ
Kim, J
Diaferio, A
Zahid, HJ
Berlind, P
Calkins, M
Tokarz, S
Moran, S
AF Hwang, Ho Seong
Geller, Margaret J.
Park, Changbom
Fabricant, Daniel G.
Kurtz, Michael J.
Rines, Kenneth J.
Kim, Juhan
Diaferio, Antonaldo
Zahid, H. Jabran
Berlind, Perry
Calkins, Michael
Tokarz, Susan
Moran, Sean
TI HECTOMAP AND HORIZON RUN 4: DENSE STRUCTURES AND VOIDS IN THE REAL AND
SIMULATED UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: statistics; large-scale structure of
universe; methods: numerical; methods: observational; surveys
ID DIGITAL SKY SURVEY; LARGE-SCALE STRUCTURE; OSCILLATION SPECTROSCOPIC
SURVEY; GALAXY REDSHIFT SURVEY; BARYON ACOUSTIC-OSCILLATIONS; N-BODY
SIMULATIONS; DARK-MATTER HALOES; WEAK-LENSING MAPS; FIBER-FED
SPECTROGRAPH; LUMINOUS RED GALAXIES
AB HectoMAP is a dense redshift survey of red galaxies covering a 53 deg(2) strip of the northern sky. HectoMAP is 97% complete for galaxies with r < 20.5, (g-r) > 1.0, and (r -i) > 0.5. The survey enables tests of the physical properties of large-scale structure at intermediate redshift against cosmological models. We use the Horizon Run 4, one of the densest and largest cosmological simulations based on the standard. Cold Dark Matter (Lambda CDM) model, to compare the physical properties of observed large-scale structures with simulated ones in a volume-limited sample covering 8 x 10(6) h(-3) Mpc(3) in the redshift range 0.22 < z < 0.44. We apply the same criteria to the observations and simulations to identify over-and under-dense large-scale features of the galaxy distribution. The richness and size distributions of observed over-dense structures agree well with the simulated ones. Observations and simulations also agree for the volume and size distributions of under-dense structures, voids. The properties of the largest over-dense structure and the largest void in HectoMAP are well within the distributions for the largest structures drawn from 300 Horizon Run 4 mock surveys. Overall the size, richness and volume distributions of observed large-scale structures in the redshift range 0.22 < z < 0.44 are remarkably consistent with predictions of the standard Lambda CDM model.
C1 [Hwang, Ho Seong; Geller, Margaret J.; Fabricant, Daniel G.; Kurtz, Michael J.; Zahid, H. Jabran; Berlind, Perry; Calkins, Michael; Tokarz, Susan; Moran, Sean] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Hwang, Ho Seong; Park, Changbom] Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 02455, South Korea.
[Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
[Kim, Juhan] Korea Inst Adv Study, Ctr Adv Computat, 85 Hoegiro, Seoul 02455, South Korea.
[Diaferio, Antonaldo] Univ Torino, Dipartimento Fis, V Pietro Giuria 1, I-10125 Turin, Italy.
[Diaferio, Antonaldo] INFN, Sez Torino, V Pietro Giuria 1, I-10125 Turin, Italy.
RP Hwang, HS; Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Hwang, HS (reprint author), Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 02455, South Korea.
EM hhwang@kias.re.kr; mgeller@cfa.harvard.edu
FU Smithsonian Institution; Clay Postdoctoral Fellowship; Supercomputing
Center/Korea Institute of Science and Technology Information
[KSC-2013-G2-003]; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy Office of Science; University of
Arizona; Brazilian Participation Group; Brookhaven National Laboratory;
Carnegie Mellon University; University of Florida; French Participation
Group; German Participation Group; Harvard University; Instituto de
Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation
Group; Johns Hopkins University; Lawrence Berkeley National Laboratory;
Max Planck Institute for Astrophysics; Max Planck Institute for
Extraterrestrial Physics; New Mexico State University; New York
University; Ohio State University; Pennsylvania State University;
University of Portsmouth; Princeton University; Spanish Participation
Group; University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; University of Washington; Yale University;
National Aeronautics and Space Administration
FX We thank the referee for a helpful and prompt report. The Smithsonian
Institution supports the research of MJG, DGF, MJK, PB, MC, ST, and SM.
HJZ is supported by the Clay Postdoctoral Fellowship. This work was
supported by the Supercomputing Center/Korea Institute of Science and
Technology Information with supercomputing resources including technical
support (KSC-2013-G2-003). We thank Korea Institute for Advanced Study
for providing computing resources (KIAS Center for Advanced Computation)
for this work. Funding for SDSS-III has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory, Carnegie
Mellon University, University of Florida, the French Participation
Group, the German Participation Group, Harvard University, the Instituto
de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University. This research has made use of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
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PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800072
ER
PT J
AU Kamble, A
Margutti, R
Soderberg, AM
Chakraborti, S
Fransson, C
Chevalier, R
Powell, D
Milisavljevic, D
Parrent, J
Bietenholz, M
AF Kamble, Atish
Margutti, Raffaella
Soderberg, Alicia M.
Chakraborti, Sayan
Fransson, Claes
Chevalier, Roger
Powell, Diana
Milisavljevic, Dan
Parrent, Jerod
Bietenholz, Michael
TI PROGENITORS OF TYPE IIb SUPERNOVAE IN THE LIGHT OF RADIO AND X-RAYS FROM
SN 2013df
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiation mechanisms: non-thermal; radio continuum: general; supernovae:
general; supernovae: individual (SN 2013df, SN 1993J)
ID CORE-COLLAPSE SUPERNOVAE; IB SUPERNOVAE; MASS-LOSS; SUPERGIANT
PROGENITOR; OBSERVATIONS REVEAL; COMPACT PROGENITOR; BINARY COMPANION;
SHOCK BREAKOUT; 1993J; EMISSION
AB We present radio and X-ray observations of the nearby SN IIb 2013df in NGC 4414 from 10 to 250 days after the explosion. The radio emission showed a peculiar steep-to-shallow spectral evolution. We present a model in which inverse Compton cooling of synchrotron emitting electrons can account for the observed spectral and light curve evolution. A significant mass-loss rate, (M) over dot approximate to 8 x 10(-5) M-circle dot yr(-1) for a wind velocity of 10 km s(-1), is estimated from the detailed modeling of radio and X-ray emission, which are primarily due to synchrotron and bremsstrahlung, respectively. We show that SN 2013df is similar to SN 1993J in various ways. The shock wave speed of SN 2013df was found to be average among the radio supernovae; v(sh)/c similar to 0.07. We did not find any significant deviation from smooth decline in the light curve of SN 2013df. One of the main results of our self-consistent multiband modeling is the significant deviation from energy equipartition between magnetic fields and relativistic electrons behind the shock. We estimate epsilon(e) = 200 epsilon(B). In general for SNe IIb, we find that the presence of bright optical cooling envelope emission is linked with free-free radio absorption and bright thermal X-ray emission. This finding suggests that more extended progenitors, similar to that of SN 2013df, suffer from substantial mass loss in the years before the supernova.
C1 [Kamble, Atish; Margutti, Raffaella; Soderberg, Alicia M.; Chakraborti, Sayan; Powell, Diana; Milisavljevic, Dan; Parrent, Jerod] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fransson, Claes] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden.
[Chevalier, Roger] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[Bietenholz, Michael] Hartebeesthoek Radio Observ, POB 443, ZA-1740 Krugersdorp, South Africa.
[Bietenholz, Michael] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada.
RP Kamble, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU David and Lucile Packard Foundation; NASA [NNX12AF90G]
FX Support for this work was provided by the David and Lucile Packard
Foundation Fellowship for Science and Engineering awarded to AMS. One of
the authors, R.A.C., acknowledges NASA grant NNX12AF90G. We thank Enrico
Ramirez-Ruiz, Nathan Sanders and Lorenzo Sironi for helpful discussions.
The authors would like to thank the anonymous referee for his
constrictive criticism which helped improve the quality of the article.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 111
DI 10.3847/0004-637X/818/2/111
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800010
ER
PT J
AU Rawls, ML
Gaulme, P
McKeever, J
Jackiewicz, J
Orosz, JA
Corsaro, E
Beck, PG
Mosser, B
Latham, DW
Latham, CA
AF Rawls, Meredith L.
Gaulme, Patrick
McKeever, Jean
Jackiewicz, Jason
Orosz, Jerome A.
Corsaro, Enrico
Beck, Paul G.
Mosser, Benoit
Latham, David W.
Latham, Christian A.
TI KIC 9246715: THE DOUBLE RED GIANT ECLIPSING BINARY WITH ODD OSCILLATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; stars: activity; stars: evolution; stars:
fundamental parameters; stars: individual (KIC 9246715); stars:
oscillations (including pulsations)
ID SOLAR-LIKE OSCILLATIONS; STELLAR ASTROPHYSICS MESA; LIMB-DARKENING
COEFFICIENTS; SPACE-BASED PHOTOMETRY; KEPLER-DATA; RADIUS DETERMINATION;
MODEL ATMOSPHERES; SCALING RELATIONS; FRAUNHOFER LINES; CORE STRUCTURE
AB We combine Kepler photometry with ground-based spectra to present a comprehensive dynamical model of the double red giant eclipsing binary KIC 9246715. While the two stars are very similar in mass (M-1 = 2.171(-0.008)(+0.006) M-circle dot, M-2 = 2.149(-0.008)(+0.006) M-circle dot) and radius (R-1 = 8.37(-0.07)(+0.03) R-circle dot, R-2 = 8.30(-0.03)(+0.04) R-circle dot), an asteroseismic analysis finds one main set of solar-like oscillations with unusually low-amplitude, wide modes. A second set of oscillations from the other star may exist, but this marginal detection is extremely faint. Because the two stars are nearly twins, KIC 9246715 is a difficult target for a precise test of the asteroseismic scaling relations, which yield M = 2.17 +/- 0.14 M-circle dot and R = 8.26 +/- 0.18 R-circle dot. Both stars are consistent with the inferred asteroseismic properties, but we suspect the main oscillator is Star 2 because it is less active than Star 1. We find evidence for stellar activity and modest tidal forces acting over the 171 day eccentric orbit, which are likely responsible for the essential lack of solar-like oscillations in one star and weak oscillations in the other. Mixed modes indicate the main oscillating star is on the secondary red clump (a core-He-burning star), and stellar evolution modeling supports this with a coeval history for a pair of red clump stars. This system is a useful case study and paves the way for a detailed analysis of more red giants in eclipsing binaries, an important benchmark for asteroseismology.
C1 [Rawls, Meredith L.; Gaulme, Patrick; McKeever, Jean; Jackiewicz, Jason] New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.
[Gaulme, Patrick] Apache Point Observ, 2001 Apache Point Rd,POB 59, Sunspot, NM 88349 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 91945 USA.
[Corsaro, Enrico; Beck, Paul G.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA,DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Corsaro, Enrico] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Corsaro, Enrico] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Mosser, Benoit] Univ Paris Diderot, Univ Paris 06, PSL Res Univ, LESIA,Observ Paris,CNRS, F-92195 Meudon, France.
[Latham, David W.; Latham, Christian A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Rawls, ML (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.
EM mrawls@nmsu.edu
OI Rawls, Meredith/0000-0003-1305-7308
FU New Mexico Space Grant Council; NASA ADAP [NNX14AR85G]; European
Community [312844, 269194]; CNES; NASA [NNX13AB58A]; Smithsonian
Astrophysical Observatory; NASA Science Mission directorate
FX This paper was written collaboratively on the web with Authorea at
authorea.com/2409. M.L.R. thanks the New Mexico Space Grant Council for
support, D. Chojnowski for assistance with APOGEE, D. Muna for the
SciCoder workshop, and L.C. Mayorga for programming assistance. J.J.
acknowledges support from NASA ADAP grant NNX14AR85G. E.C. and P.B.
received funding from the European Community's Seventh Framework
Programme [FP7/2007-2013] under grant agreements 312844 (SPACE-INN) and
269194 (IRSES/ASK). P.B. also received funding from CNES grants at CEA.
D.W.L. acknowledges partial support from NASA's Kepler Mission under
Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical
Observatory. We thank Leo Girardi and the anonymous referee for valuable
feedback and Kresimir Pavlovski for useful discussions. This paper uses
data from the Apache Point Observatory 3.5-m telescope, which is owned
and operated by the Astrophysical Research Consortium, and data
collected by the Kepler mission, which is funded by the NASA Science
Mission directorate. This research made use of Astropy (Robitaille et
al. 2013), PyAstronomy (github.com/sczesla/PyAstronomy), PyKE (Still &
Barclay 2012), NASA's ADS Bibliographic Services, and the AstroBetter
blog and wiki.
NR 79
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
PD FEB 20
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AR 108
DI 10.3847/0004-637X/818/2/108
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800007
ER
PT J
AU Rodigas, TJ
Arriagada, P
Faherty, J
Anglada-Escude, G
Kaib, N
Butler, RP
Shectman, S
Weinberger, A
Males, JR
Morzinski, KM
Close, LM
Hinz, PM
Crane, JD
Thompson, I
Teske, J
Diaz, M
Minniti, D
Lopez-Morales, M
Adams, FC
Boss, AP
AF Rodigas, Timothy J.
Arriagada, Pamela
Faherty, Jackie
Anglada-Escude, Guillem
Kaib, Nathan
Butler, R. Paul
Shectman, Stephen
Weinberger, Alycia
Males, Jared R.
Morzinski, Katie M.
Close, Laird M.
Hinz, Philip M.
Crane, Jeffrey D.
Thompson, Ian
Teske, Johanna
Diaz, Matias
Minniti, Dante
Lopez-Morales, Mercedes
Adams, Fred C.
Boss, Alan P.
TI MagAO IMAGING OF LONG-PERIOD OBJECTS (MILO). I. A BENCHMARK M DWARF
COMPANION EXCITING A MASSIVE PLANET AROUND THE SUN-LIKE STAR HD 7449
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; instrumentation: adaptive optics; planetary systems;
stars: individual (HD 7449); techniques: high angular resolution;
techniques: radial velocities
ID SOLAR-TYPE STARS; EVOLUTIONARY MODELS; EXTRASOLAR PLANETS;
RADIAL-VELOCITY; GIANT PLANET; SUPER-EARTH; EXOPLANET; SYSTEMS; ORBITS;
BINARIES
AB We present high-contrast Magellan adaptive optics images of HD 7449, a Sun-like star with one planet and a long-term radial velocity (RV) trend. We unambiguously detect the source of the long-term trend from 0.6-2.15 mu m. at a separation of similar to 0.'' 54. We use the object's colors and spectral energy distribution to show that it is most likely an M4-M5 dwarf (mass similar to 0.1-0.2 M-circle dot) at the same distance as the primary and is therefore likely bound. We also present new RVs measured with the Magellan/MIKE and Planet Finder Spectrograph spectrometers and compile these with archival data from CORALIE and HARPS. We use a new Markov chain Monte Carlo procedure to constrain both the mass (>0.17 M-circle dot at 99% confidence) and semimajor axis (similar to 18 AU) of the M dwarf companion (HD 7449B). We also refine the parameters of the known massive planet (HD 7449Ab), finding that its minimum mass is 1.09(-0.19)(+0.52) M-J, its semimajor axis is 2.33(-0.02)(+0.01) AU, and its eccentricity is 0.8(-0.06)(+0.08). We use N-body simulations to constrain the eccentricity of HD 7449B to less than or similar to 0.5. The M dwarf may be inducing Kozai oscillations on the planet, explaining its high eccentricity. If this is the case and its orbit was initially circular, the mass of the planet would need to be less than or similar to 1.5 M-J. This demonstrates that strong constraints on known planets can be made using direct observations of otherwise undetectable long-period companions.
C1 [Rodigas, Timothy J.; Arriagada, Pamela; Faherty, Jackie; Butler, R. Paul; Weinberger, Alycia; Teske, Johanna; Boss, Alan P.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Anglada-Escude, Guillem] Univ London, Sch Phys & Astron, 327 Mile End Rd, London, England.
[Kaib, Nathan] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Shectman, Stephen; Crane, Jeffrey D.; Thompson, Ian; Diaz, Matias] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Males, Jared R.; Morzinski, Katie M.; Close, Laird M.; Hinz, Philip M.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Diaz, Matias] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[Minniti, Dante] Univ Andres Bello, Dept Ciencias Fis, Campus La Casona,Fernndez Concha 700, Santiago, Chile.
[Minniti, Dante] Millennium Inst Astrophys, Ave Vicua Mackenna 4860, Santiago 7820436, Chile.
[Minniti, Dante] Vatican Observ, I-00120 Vatican City, Vatican.
[Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA.
[Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Rodigas, TJ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM trodigas@carnegiescience.edu
RI Butler, Robert/B-1125-2009;
OI Anglada Escude, Guillem/0000-0002-3645-5977
FU NASA from the Space Telescope Science Institute [HST-HF2-51366.001-A];
NASA [NAS5-26555]; BASAL CATA Center for Astrophysics and Associated
Technologies [PFB-06]; Ministry for the Economy, Development, and
Tourism's Programa Iniciativa Cientfica Milenio [IC120009]; FONDECYT
[1130196]
FX We thank Andrew Tribick and Alexander Venner for notifying us of a unit
conversion mistake prior to the article's publication. T.J.R.
acknowledges support for Program number HST-HF2-51366.001-A, provided by
NASA through a Hubble Fellowship grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
Support for D.M. is provided by the BASAL CATA Center for Astrophysics
and Associated Technologies through grant PFB-06, by the Ministry for
the Economy, Development, and Tourism's Programa Iniciativa Cientfica
Milenio through grant IC120009, awarded to the Millennium Institute of
Astrophysics (MAS), and by FONDECYT No. 1130196.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 106
DI 10.3847/0004-637X/818/2/106
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800005
ER
PT J
AU Smith, RK
Valencic, LA
Corrales, L
AF Smith, Randall K.
Valencic, Lynne A.
Corrales, Lia
TI THE IMPACT OF ACCURATE EXTINCTION MEASUREMENTS FOR X-RAY SPECTRAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; methods: data analysis; X-rays: ISM
ID INTERSTELLAR DUST GRAINS; XMM-NEWTON; BINARY EXO-0748-676; NEUTRON-STAR;
EXO 0748-676; SCATTERING; HALOS; ASTROPHYSICS; ABSORPTION
AB Interstellar extinction includes both absorption and scattering of photons from interstellar gas and dust grains, and it has the effect of altering a source's spectrum and its total observed intensity. However, while multiple absorption models exist, there are no useful scattering models in standard X-ray spectrum fitting tools, such as XSPEC. Nonetheless, X-ray halos, created by scattering from dust grains, are detected around even moderately absorbed sources, and the impact on an observed source spectrum can be significant, if modest, compared to direct absorption. By convolving the scattering cross section with dust models, we have created a spectral model as a function of energy, type of dust, and extraction region that can be used with models of direct absorption. This will ensure that the extinction model is consistent and enable direct connections to be made between a source's X-ray spectral fits and its UV/optical extinction.
C1 [Smith, Randall K.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA.
[Corrales, Lia] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,37-241, Cambridge, MA 02139 USA.
RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Valencic, LA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA.
EM lynne.a.valencic@nasa.gov
FU Chandra grant [TM4-15002X]
FX The authors thank the anonymous referee for prompt and helpful comments
that significantly improved the work. We also thank Sebastian Heinz for
reviewing the xscat code and helping to debug it. Randall Smith
gratefully acknowledges helpful discussions and overall inspiration to
work on X-ray scattering from Eli Dwek. Financial support for this work
was made possible by Chandra grant TM4-15002X.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
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AR 143
DI 10.3847/0004-637X/818/2/143
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800042
ER
PT J
AU Snios, B
Kharchenko, V
Lisse, CM
Wolk, SJ
Dennerl, K
Combi, MR
AF Snios, Bradford
Kharchenko, Vasili
Lisse, Carey M.
Wolk, Scott J.
Dennerl, Konrad
Combi, Michael R.
TI CHANDRA OBSERVATIONS OF COMETS C/2012 S1 (ISON) AND C/2011 L4
(PanSTARRS)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: individual (Comet S1/ISON, Comet L4/PanSTARRS); solar wind;
techniques: spectroscopic; X-rays: general
ID X-RAY-EMISSION; SOLAR-WIND IONS; SELECTIVE ELECTRON-CAPTURE;
CHARGE-TRANSFER; ULTRAVIOLET EMISSION; WATER PRODUCTION; ATOMIC
DATABASE; SLOW COLLISIONS; MINOR IONS; HEAVY-IONS
AB We present our results on the Chandra X-ray Observatory Advanced CCD Imaging Spectrometer (ACIS) observations of the bright Oort Cloud comets C/2012 S1 (ISON) and C/2011 L4 (PanSTARRS). ISON was observed between 2013 October 31-November 06 during variable speed solar wind (SW), and PanSTARRS was observed between 2013 April 17-23 during fast SW. ISON produced an extended parabolic X-ray morphology consistent with a collisionally thick coma, while PanSTARRS demonstrated only a diffuse X-ray-emitting region. We consider these emissions to be from charge exchange (CX) and model each comet's emission spectrum from first principles accordingly. Our model agrees with the observational spectra and also generates composition ratios for heavy, highly charged SW ions interacting with the cometary atmosphere. We compare our derived SW ion compositions to observational data and find a strong agreement between them. These results further demonstrate the utility of CX emissions as a remote diagnostics tool of both astrophysical plasma interaction and SW composition. In addition, we observe potential soft X-ray emissions via ACIS around 0.2 keV from both comets that are correlated in intensity to the hard X-ray emissions between 0.4-1.0 keV. We fit our CX model to these emissions, but our lack of a unique solution at low energies makes it impossible to conclude if they are cometary CX in origin. Finally, we discuss probable emission mechanism sources for the soft X-rays and explore new opportunities these findings present in understanding cometary emission processes via Chandra.
C1 [Snios, Bradford; Kharchenko, Vasili] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Observ Ctr, Cambridge, MA 02138 USA.
[Dennerl, Konrad] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Combi, Michael R.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
RP Snios, B (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
RI Lisse, Carey/B-7772-2016; Combi, Michael/J-1697-2012
OI Lisse, Carey/0000-0002-9548-1526; Snios, Bradford /0000-0002-4900-928X;
Combi, Michael/0000-0002-9805-0078
FU NASA [NNX10AB88G]; Chandra grant [GO4-15001A]
FX We would like to acknowledge National Oceanic and Atmospheric
Administration for their Advanced Composition Explorer data. The work of
B.S. and V.K. on this project has been supported by NASA (Grant
NNX10AB88G). The work of C.L. has been supported by Chandra grant
GO4-15001A.
NR 48
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 199
DI 10.3847/0004-637X/818/2/199
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800098
ER
PT J
AU Trott, CM
Pindor, B
Procopio, P
Wayth, RB
Mitchell, DA
McKinley, B
Tingay, SJ
Barry, N
Beardsley, AP
Bernardi, G
Bowman, JD
Briggs, F
Cappallo, RJ
Carroll, P
de Oliveira-Costa, A
Dillon, JS
Ewall-Wice, A
Feng, L
Greenhill, LJ
Hazelton, BJ
Hewitt, JN
Hurley-Walker, N
Johnston-Hollitt, M
Jacobs, DC
Kaplan, DL
Kim, HS
Lenc, E
Line, J
Loeb, A
Lonsdale, CJ
Morales, MF
Morgan, E
Neben, AR
Thyagarajan, N
Oberoi, D
Offringa, AR
Ord, SM
Paul, S
Pober, JC
Prabu, T
Riding, J
Shankar, NU
Sethi, SK
Srivani, KS
Subrahmanyan, R
Sullivan, IS
Tegmark, M
Webster, RL
Williams, A
Williams, CL
Wu, C
Wyithe, JSB
AF Trott, C. M.
Pindor, B.
Procopio, P.
Wayth, R. B.
Mitchell, D. A.
McKinley, B.
Tingay, S. J.
Barry, N.
Beardsley, A. P.
Bernardi, G.
Bowman, Judd D.
Briggs, F.
Cappallo, R. J.
Carroll, P.
de Oliveira-Costa, A.
Dillon, Joshua S.
Ewall-Wice, A.
Feng, L.
Greenhill, L. J.
Hazelton, B. J.
Hewitt, J. N.
Hurley-Walker, N.
Johnston-Hollitt, M.
Jacobs, Daniel C.
Kaplan, D. L.
Kim, H. S.
Lenc, E.
Line, J.
Loeb, A.
Lonsdale, C. J.
Morales, M. F.
Morgan, E.
Neben, A. R.
Thyagarajan, Nithyanandan
Oberoi, D.
Offringa, A. R.
Ord, S. M.
Paul, S.
Pober, J. C.
Prabu, T.
Riding, J.
Shankar, N. Udaya
Sethi, Shiv K.
Srivani, K. S.
Subrahmanyan, R.
Sullivan, I. S.
Tegmark, M.
Webster, R. L.
Williams, A.
Williams, C. L.
Wu, C.
Wyithe, J. S. B.
TI CHIPS: THE COSMOLOGICAL H I POWER SPECTRUM ESTIMATOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Astronomical instrumentation, methods and techniques; early universe;
methods: statistical; techniques: interferometric
ID 21 CM EPOCH; MURCHISON WIDEFIELD ARRAY; RADIO OBSERVATIONS; FOREGROUND
REMOVAL; REIONIZATION; LOFAR; SIMULATIONS; SENSITIVITY; CALIBRATION;
LIMITATIONS
AB Detection of the cosmological neutral hydrogen signal from the Epoch of Reionization (EoR). and estimation of its basic physical parameters. are. principal scientific aims of many current low-frequency radio telescopes. Here we describe the Cosmological H I Power Spectrum Estimator (CHIPS), an algorithm developed and implemented with data from the Murchison Widefield Array, to compute the two-dimensional and spherically-averaged power spectrum of brightness temperature fluctuations. The principal motivations for CHIPS are the application of realistic instrumental and foreground models to form the optimal estimator, thereby maximizing the likelihood of unbiased signal estimation, and allowing a full covariant understanding of the outputs. CHIPS employs an inverse-covariance weighting of the data through the maximum likelihood estimator, thereby allowing use of the full parameter space for signal estimation ("foreground suppression"). We describe the motivation for the algorithm, implementation, application to real and simulated data, and early outputs. Upon application to a set of 3 hr of data, we set a 2 sigma upper limit on the EoR dimensionless power at k = 0.05 h Mpc(-1) of Delta(2)(k) < 7.6 x 10(4) mK(2) in the redshift range z = [6.2-6.6], consistent with previous estimates.
C1 [Trott, C. M.; Wayth, R. B.; Tingay, S. J.; Hurley-Walker, N.; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Trott, C. M.; Pindor, B.; Procopio, P.; Wayth, R. B.; Mitchell, D. A.; McKinley, B.; Tingay, S. J.; Briggs, F.; Kim, H. S.; Lenc, E.; Line, J.; Offringa, A. R.; Ord, S. M.; Riding, J.; Subrahmanyan, R.; Webster, R. L.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia.
[Pindor, B.; Procopio, P.; McKinley, B.; Kim, H. S.; Line, J.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Mitchell, D. A.] CSIRO Astron & Space Sci CASS, POB 76, Epping, NSW 1710, Australia.
[Barry, N.; Beardsley, A. P.; Carroll, P.; Hazelton, B. J.; Morales, M. F.; Pober, J. C.; Sullivan, I. S.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Beardsley, A. P.; Bowman, Judd D.; Jacobs, Daniel C.; Thyagarajan, Nithyanandan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Bernardi, G.] SKA SA, Pk Rd, ZA-7405 Pinelands, South Africa.
[Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Bernardi, G.; Greenhill, L. J.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Cappallo, R. J.; Lonsdale, C. J.] MIT, Haystack Observ, Westford, MA 01886 USA.
[de Oliveira-Costa, A.; Dillon, Joshua S.; Ewall-Wice, A.; Feng, L.; Hewitt, J. N.; Morgan, E.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Hazelton, B. J.] Univ Washington, eSci Inst, Seattle, WA 98195 USA.
[Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Kaplan, D. L.] Univ Wisconsin Milwaukee, Dept Phys, Milwaukee, WI 53201 USA.
[Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands.
[Paul, S.; Prabu, T.; Shankar, N. Udaya; Sethi, Shiv K.; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Pober, J. C.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wu, C.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
RP Trott, CM (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
EM cathryn.trott@curtin.edu.au
RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar ,
N/D-4901-2012; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012;
OI Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766;
Lenc, Emil/0000-0002-9994-1593; KIM, HANSIK/0000-0002-5507-5769; Wyithe,
Stuart/0000-0001-7956-9758; /0000-0002-0086-7363; Pober,
Jonathan/0000-0002-3492-0433
FU Australian Research Council [DE140100316]; U.S. National Science
Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884];
Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air
Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky
Astrophysics (an Australian Research Council Centre of Excellence)
[CE110001020]; Smithsonian Astrophysical Observatory; MIT School of
Science; Raman Research Institute; Australian National University;
Victoria University of Wellington from the New Zealand Ministry of
Economic Development [MED-E1799]; Victoria University of Wellington from
the IBM [MED-E1799]; Australian Federal Government via the Commonwealth
Scientific and Industrial Research Organisation (CSIRO); National
Collaborative Research Infrastructure Strategy, Education Investment
Fund; Australia India Strategic Research Fund; Astronomy Australia
Limited; Australian Government; Government of Western Australia;
Swinburne Government; NVIDIA at Harvard University; International Centre
for Radio Astronomy Research (ICRAR); Western Australian State
Government
FX We thank the referee for a very thorough reading of the manuscript. and
many excellent suggestions to improve its clarity. This research was
supported under Australian Research Council's Discovery Early Career
Researcher funding scheme (project number DE140100316). This scientific
work makes use of the Murchison Radio-astronomy Observatory, operated by
CSIRO. We acknowledge the Wajarri Yamatji people as the traditional
owners of the Observatory site. Support for the MWA comes from the U.S.
National Science Foundation (grants AST-0457585, PHY-0835713,
CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF
grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific
Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics
(an Australian Research Council Centre of Excellence funded by grant
CE110001020). Support is also provided by the Smithsonian Astrophysical
Observatory, the MIT School of Science, the Raman Research Institute,
the Australian National University, and the Victoria University of
Wellington (via grant MED-E1799 from the New Zealand Ministry of
Economic Development and an IBM Shared University Research Grant). The
Australian Federal Government provides additional support via the
Commonwealth Scientific and Industrial Research Organisation (CSIRO),
National Collaborative Research Infrastructure Strategy, Education
Investment Fund, and the Australia India Strategic Research Fund, and
Astronomy Australia Limited, under contract to Curtin University. This
work was supported by resources provided by the Pawsey Supercomputing
Centre with funding from the Australian Government and the Government of
Western Australia. This work was supported by resources awarded under
Astronomy Australia Ltds merit allocation scheme on the gSTAR national
facility at Swinburne University of Technology. gSTAR is funded by
Swinburne and the Australian Governments Education Investment Fund. We
acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative
Computing and the CUDA Center for Excellence sponsored by NVIDIA at
Harvard University, and the International Centre for Radio Astronomy
Research (ICRAR), a Joint Venture of Curtin University and The
University of Western Australia, funded by the Western Australian State
Government.
NR 57
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 139
DI 10.3847/0004-637X/818/2/139
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800038
ER
PT J
AU van Weeren, RJ
Brunetti, G
Bruggen, M
Andrade-Santos, F
Ogrean, GA
Williams, WL
Rottgering, HJA
Dawson, WA
Forman, WR
de Gasperin, F
Hardcastle, MJ
Jones, C
Miley, GK
Rafferty, DA
Rudnick, L
Sabater, J
Sarazin, CL
Shimwell, TW
Bonafede, A
Best, PN
Birzan, L
Cassano, R
Chyzy, KT
Croston, JH
Dijkema, TJ
Ensslin, T
Ferrari, C
Heald, G
Hoeft, M
Horellou, C
Jarvis, MJ
Kraft, RP
Mevius, M
Intema, HT
Murray, SS
Orru, E
Pizzo, R
Sridhar, SS
Simionescu, A
Stroe, A
van der Tol, S
White, GJ
AF van Weeren, R. J.
Brunetti, G.
Brueggen, M.
Andrade-Santos, F.
Ogrean, G. A.
Williams, W. L.
Rottgering, H. J. A.
Dawson, W. A.
Forman, W. R.
de Gasperin, F.
Hardcastle, M. J.
Jones, C.
Miley, G. K.
Rafferty, D. A.
Rudnick, L.
Sabater, J.
Sarazin, C. L.
Shimwell, T. W.
Bonafede, A.
Best, P. N.
Birzan, L.
Cassano, R.
Chyzy, K. T.
Croston, J. H.
Dijkema, T. J.
Ensslin, T.
Ferrari, C.
Heald, G.
Hoeft, M.
Horellou, C.
Jarvis, M. J.
Kraft, R. P.
Mevius, M.
Intema, H. T.
Murray, S. S.
Orru, E.
Pizzo, R.
Sridhar, S. S.
Simionescu, A.
Stroe, A.
van der Tol, S.
White, G. J.
TI LOFAR, VLA, AND CHANDRA OBSERVATIONS OF THE TOOTHBRUSH GALAXY CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (RX J0603.3+4214); galaxies: clusters:
intracluster medium; large-scale structure of universe; radiation
mechanisms: non-thermal; X-rays: galaxies: clusters
ID COSMOLOGICAL SHOCK-WAVES; DIFFUSE RADIO-EMISSION; LARGE-SCALE STRUCTURE;
NONTHERMAL ELECTRON ACCELERATION; COSMIC-RAY PROTONS; X-RAY; COMA
CLUSTER; LOW-FREQUENCY; BOW SHOCK; GAMMA-RAY
AB We present deep LOFAR observations between 120 and 181 MHz of the "Toothbrush" (RX J0603.3+ 4214), a cluster that contains one of the brightest radio relic sources known. Our LOFAR observations exploit a new and novel calibration scheme to probe 10 times deeper than any previous study in this relatively unexplored part of the spectrum. The LOFAR observations, when combined with VLA, GMRT, and Chandra X-ray data, provide new information about the nature of cluster merger shocks and their role in re-accelerating relativistic particles. We derive a spectral index of alpha = -0.8 +/- 0.1 at the northern edge of the main radio relic, steepening toward the south to alpha approximate to-2. The spectral index of the radio halo is remarkably uniform (alpha = -1.16, with an intrinsic scatter of <= 0.04). The observed radio relic spectral index gives a Mach number of M = 2.8(-0.3)(+0.5), assuming diffusive shock acceleration. However, the gas density jump at the northern edge of the large radio relic implies a much weaker shock (M approximate to 1.2, with an upper limit of M approximate to 1.5). The discrepancy between the Mach numbers calculated from the radio and X-rays can be explained if either (i) the relic traces a complex shock surface along the line of sight, or (ii) if the radio relic emission is produced by a re-accelerated population of fossil particles from a radio galaxy. Our results highlight the need for additional theoretical work and numerical simulations of particle acceleration and re-acceleration at cluster merger shocks.
C1 [van Weeren, R. J.; Andrade-Santos, F.; Ogrean, G. A.; Forman, W. R.; Jones, C.; Kraft, R. P.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Brunetti, G.; Cassano, R.] Ist Radioastron, INAF, Via Gobetti 101, I-40129 Bologna, Italy.
[Brueggen, M.; de Gasperin, F.; Rafferty, D. A.; Bonafede, A.; Birzan, L.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Williams, W. L.; Rottgering, H. J. A.; de Gasperin, F.; Miley, G. K.; Shimwell, T. W.; Intema, H. T.; Stroe, A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Williams, W. L.; Dijkema, T. J.; Heald, G.; Mevius, M.; Orru, E.; Pizzo, R.; Sridhar, S. S.; van der Tol, S.] ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Williams, W. L.; Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Dawson, W. A.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA.
[Rudnick, L.] Univ Minnesota, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA.
[Sabater, J.; Best, P. N.] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Chyzy, K. T.] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Ensslin, T.] Max Planck Inst Astrophys, Karl Schwarzschildstr 1, D-85741 Garching, Germany.
[Ferrari, C.] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Heald, G.; Sridhar, S. S.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Hoeft, M.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
[Horellou, C.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Jarvis, M. J.] Oxford Astrophys, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
[Jarvis, M. J.] Univ Western Cape, ZA-7535 Bellville, South Africa.
[Intema, H. T.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA.
[Simionescu, A.] JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[White, G. J.] Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England.
RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rvanweeren@cfa.harvard.edu
RI Intema, Huib/D-1438-2012;
OI Intema, Huib/0000-0002-5880-2730; Seethapuram Sridhar,
Sarrvesh/0000-0002-7587-4779; Sabater, Jose/0000-0003-1149-6294; van
Weeren, Reinout/0000-0002-0587-1660; Hardcastle,
Martin/0000-0003-4223-1117
FU NASA - Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; National
Aeronautics and Space Administration through Chandra Award - Chandra
X-ray Observatory Center [NAS8-03060, GO3-14138X]; NASA through a Hubble
Fellowship - Space Telescope Science Institute [HST-HF2-51345.001-A,
NAS5-26555]; Alexander von Humboldt Foundation; PRIN-INAF; Smithsonian
Institution; Chandra grant [G03-14131X]; Agence Nationale pour la
Recherche, MAGELLAN project [ANR-14-CE23-0004-01]; NSF [AST-1211595];
U.S. DOE by LLNL [DE-AC52-07NA27344]
FX We would like to thank the anonymous referee for useful comments. RJW
was supported by NASA through the Einstein Postdoctoral grant number
PF2-130104 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO3-14138X issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060. GAO acknowledges support by NASA through a Hubble Fellowship
grant HST-HF2-51345.001-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Incorporated, under NASA contract NAS5-26555. GB
acknowledges support from the Alexander von Humboldt Foundation. GB and
RC acknowledge support from PRIN-INAF 2014. WRF, CJ, and FA-S
acknowledge support from the Smithsonian Institution. FA-S acknowledges
support from Chandra grant G03-14131X. CF acknowledges support by the
Agence Nationale pour la Recherche, MAGELLAN project,
ANR-14-CE23-0004-01. Partial support for LR is provided by NSF Grant
AST-1211595 to the University of Minnesota. Part of this work performed
under the auspices of the U.S. DOE by LLNL under Contract
DE-AC52-07NA27344. LOFAR, the Low Frequency Array designed and
constructed by ASTRON, has facilities in several countries, that are
owned by various parties (each with their own funding sources), and that
are collectively operated by the International LOFAR Telescope (ILT)
foundation under a joint scientific policy. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. We thank
the staff of the GMRT that made these observations possible. GMRT is run
by the National Centre for Radio Astrophysics of the Tata Institute of
Fundamental Research. The Open University is incorporated by Royal
Charter (RC 000391), an exempt charity in England & Wales and a charity
registered in Scotland (SC 038302). The Open University is authorized
and regulated by the Financial Conduct Authority.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 204
DI 10.3847/0004-637X/818/2/204
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800103
ER
PT J
AU Zuluaga, JI
Mason, PA
Cuartas-Restrepo, PA
AF Zuluaga, Jorge I.
Mason, Paul A.
Cuartas-Restrepo, Pablo A.
TI CONSTRAINING THE RADIATION AND PLASMA ENVIRONMENT OF THE KEPLER
CIRCUMBINARY HABITABLE-ZONE PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; planet-star interactions; planets and satellites:
individual (Kepler-16b, Kepler-47c, Kepler-453b); stars: activity
ID ANGULAR-MOMENTUM EVOLUTION; MAIN-SEQUENCE STARS; LOW-MASS STARS; STELLAR
X-RAY; BINARY-SYSTEMS; TERRESTRIAL PLANETS; ATMOSPHERIC MASS; ROTATION;
MODEL; PHOTOCHEMISTRY
AB The discovery of many planets using the Kepler telescope includes 10. planets orbiting eight binary stars. Three binaries, Kepler-16, Kepler-47, and Kepler-453, have at least one planet in the circumbinary habitable zone (BHZ). We constrain the level of high-energy radiation and the plasma environment in the BHZ of these systems. With this aim, BHZ limits in these Kepler binaries are calculated as a function of time, and the habitability lifetimes are estimated for hypothetical terrestrial planets and/or moons within the BHZ. With the time-dependent BHZ limits established, a self-consistent model is developed describing the evolution of stellar activity and radiation properties as proxies for stellar aggression toward planetary atmospheres. Modeling binary stellar rotation evolution, including the effect of tidal interaction between stars in binaries, is key to establishing the environment around these systems. We find that Kepler-16 and its binary analogs. provide a plasma environment favorable for the survival of atmospheres of putative Mars-sized planets and exomoons. Tides have modified the rotation of the stars in Kepler-47, making its radiation environment less harsh in comparison to the solar system. This is a good example of the mechanism first proposed by Mason et al. Kepler-453 has an environment similar to that of the solar system with slightly better than Earth radiation conditions at the inner edge of the BHZ. These results can be reproduced and even reparameterized as stellar evolution and binary tidal models progress, using our online tool http://bhmcalc.net.
C1 [Zuluaga, Jorge I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zuluaga, Jorge I.; Cuartas-Restrepo, Pablo A.] Univ Antioquia, FCEN, Inst Fis, FACom, Calle 70 52-21, Medellin, Colombia.
[Mason, Paul A.] New Mexico State Univ, DACC, Las Cruces, NM 88003 USA.
RP Zuluaga, JI (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.; Zuluaga, JI (reprint author), Univ Antioquia, FCEN, Inst Fis, FACom, Calle 70 52-21, Medellin, Colombia.
FU Estrategia de Sostenibilidad de la Universidad de Antioquia; COID/UdeA;
NMSU-DACC; Fulbright Commission, Colombia
FX We thank W. Welsh for discussions concerning the Kepler planets and N.
Haghighapor for pointing out the importance of resonances. We also thank
S. Cranmer, G. Torres, and A. Claret for discussion about their models
applied in this work. We appreciate the help of I. Baraffe, who provided
detailed stellar evolutionary models, including moment-of-inertia
calculations, required in the rotational evolution calculations. Special
thanks to the anonymous referee, who provided useful input for improving
the BHZ models and suggestions for improving the clarity of the
manuscript. J.I.Z. and P.A.C. are supported by Estrategia de
Sostenibilidad 2014-2015 de la Universidad de Antioquia and by
COID/UdeA. P.A.M. is supported by NMSU-DACC. J.I.Z. is also supported by
the Fulbright Commission, Colombia. He also thanks the
Harvard-Smithsonian Center for Astrophysics for their hospitality.
NR 90
TC 1
Z9 1
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2016
VL 818
IS 2
AR 160
DI 10.3847/0004-637X/818/2/160
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7ZS
UT WOS:000372302800059
ER
PT J
AU Abeysekara, AU
Archambault, S
Archer, A
Benbow, W
Bird, R
Buchovecky, M
Buckley, JH
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, X
Christiansen, JL
Ciupik, L
Cui, W
Dickinson, HJ
Eisch, JD
Errando, M
Falcone, A
Fegan, DJ
Feng, Q
Finley, JP
Fleischhack, H
Fortin, P
Fortson, L
Furniss, A
Gillanders, GH
Griffin, S
Grube, J
Gyuk, G
Hutten, M
Hakansson, N
Hanna, D
Holder, J
Humensky, TB
Johnson, CA
Kaaret, P
Kar, P
Kelley-Hoskins, N
Kertzman, M
Kieda, D
Krause, M
Krennrich, F
Kumar, S
Lang, MJ
Lin, TTY
Maier, G
McArthur, S
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
O'Brien, S
de Bhroithe, AO
Ong, RA
Otte, AN
Park, N
Perkins, JS
Petrashyk, A
Pohl, M
Popkow, A
Pueschel, E
Quinn, J
Ragan, K
Ratliff, G
Reynolds, PT
Richards, GT
Roache, E
Santander, M
Sembroski, GH
Shahinyan, K
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Vincent, S
Wakely, SP
Weiner, OM
Weinstein, A
Williams, DA
Zitzer, B
AF Abeysekara, A. U.
Archambault, S.
Archer, A.
Benbow, W.
Bird, R.
Buchovecky, M.
Buckley, J. H.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Christiansen, J. L.
Ciupik, L.
Cui, W.
Dickinson, H. J.
Eisch, J. D.
Errando, M.
Falcone, A.
Fegan, D. J.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortin, P.
Fortson, L.
Furniss, A.
Gillanders, G. H.
Griffin, S.
Grube, J.
Gyuk, G.
Huetten, M.
Hakansson, N.
Hanna, D.
Holder, J.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kelley-Hoskins, N.
Kertzman, M.
Kieda, D.
Krause, M.
Krennrich, F.
Kumar, S.
Lang, M. J.
Lin, T. T. Y.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
O'Brien, S.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Park, N.
Perkins, J. S.
Petrashyk, A.
Pohl, M.
Popkow, A.
Pueschel, E.
Quinn, J.
Ragan, K.
Ratliff, G.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Vincent, S.
Wakely, S. P.
Weiner, O. M.
Weinstein, A.
Williams, D. A.
Zitzer, B.
TI A SEARCH FOR BRIEF OPTICAL FLASHES ASSOCIATED WITH THE SETI TARGET KIC
8462852
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; extraterrestrial intelligence; methods: observational;
stars: individual ( KIC 8462852); techniques: photometric
ID EXTRATERRESTRIAL INTELLIGENCE; TELESCOPES; SPECTRA; STARS; VERITAS;
BURSTS; SYSTEM; OSETI
AB The F-type star KIC. 8462852 has recently been identified as an exceptional target for search for extraterrestrial intelligence (SETI) observations. We describe an analysis methodology for optical SETI, which we have used to analyze nine hours of serendipitous archival observations of KIC. 8462852 made with the VERITAS gamma-ray observatory between 2009 and 2015. No evidence of pulsed optical beacons, above a pulse intensity at the Earth of approximately 1 photon m(-2), is found. We also discuss the potential use of imaging atmospheric Cherenkov telescope arrays in searching for extremely short duration optical transients in general.
C1 [Abeysekara, A. U.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; Lin, T. T. Y.; McCann, A.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Buckley, J. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Fegan, D. J.; O'Brien, S.; Pueschel, E.; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Buchovecky, M.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Telezhinsky, I.; Vincent, S.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA.
[Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Holder, J.] Florida Inst Technol, Dept Phys & Space Sci, W Melbourne, FL 32901 USA.
[Humensky, T. B.; Nieto, D.; Petrashyk, A.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Phys Sci, Cork, Ireland.
RP Dickinson, HJ (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.; Holder, J (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.; Holder, J (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.; Holder, J (reprint author), Florida Inst Technol, Dept Phys & Space Sci, W Melbourne, FL 32901 USA.
EM hughd@iastate.edu; jholder@physics.udel.edu
RI Nieto, Daniel/J-7250-2015;
OI Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973;
Krause, Maria/0000-0001-7595-0914; Bird, Ralph/0000-0002-4596-8563
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation, and the
Smithsonian Institution, and by NSERC in Canada. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument. The VERITAS Collaboration
is grateful to Trevor Weekes for his seminal contributions and
leadership in the field of VHE gamma-ray astrophysics. and for his
interest in the wider applications of IACTs, which made this study
possible.
NR 40
TC 3
Z9 3
U1 3
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2016
VL 818
IS 2
AR L33
DI 10.3847/2041-8205/818/2/L33
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE2GK
UT WOS:000370444800012
ER
PT J
AU Cenko, SB
Cucchiara, A
Roth, N
Veilleux, S
Prochaska, JX
Yan, L
Guillochon, J
Maksym, WP
Arcavi, I
Butler, NR
Filippenko, AV
Fruchter, AS
Gezari, S
Kasen, D
Levan, AJ
Miller, JM
Pasham, DR
Ramirez-Ruiz, E
Strubbe, LE
Tanvir, NR
Tombesi, F
AF Cenko, S. Bradley
Cucchiara, Antonino
Roth, Nathaniel
Veilleux, Sylvain
Prochaska, J. Xavier
Yan, Lin
Guillochon, James
Maksym, W. Peter
Arcavi, Iair
Butler, Nathaniel R.
Filippenko, Alexei V.
Fruchter, Andrew S.
Gezari, Suvi
Kasen, Daniel
Levan, Andrew J.
Miller, Jon M.
Pasham, Dheeraj R.
Ramirez-Ruiz, Enrico
Strubbe, Linda E.
Tanvir, Nial R.
Tombesi, Francesco
TI AN ULTRAVIOLET SPECTRUM OF THE TIDAL DISRUPTION FLARE ASASSN-14li
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; stars: flare; ultraviolet: general
ID DIGITAL SKY SURVEY; NITROGEN-ENRICHED QUASARS; SUPERMASSIVE BLACK-HOLE;
MAIN-SEQUENCE STAR; DATA RELEASE; LY-ALPHA; GALAXIES; PS1-10JH; EVENTS;
ABSORPTION
AB We present a Hubble Space Telescope Space Telescope Imaging Spectrograph spectrum of ASASSN-14li, the first rest-frame ultraviolet (UV) spectrum of a tidal disruption flare (TDF). The underlying continuum is well fit by a blackbody with T-UV 3.5 x 10(4) K, an order of magnitude smaller than the temperature inferred from X-ray spectra (and significantly more precise than previous efforts based on optical and near-UV photometry). Superimposed on this blue continuum, we detect three classes of features: narrow absorption from the Milky Way (probably a high-velocity cloud), and narrow absorption and broad (similar to 2000-8000 km s(-1)) emission lines at or near the systemic host velocity. The absorption lines are blueshifted with respect to the emission lines by Delta nu = -(250-400) km s(-1). Due both to this velocity offset and the lack of common low-ionization features (Mg II, Fe II), we argue these arise from the same absorbing material responsible for the low-velocity outflow discovered at X-ray wavelengths. The broad nuclear emission lines display a remarkable abundance pattern: N III], NIV], and He II are quite prominent, while the common quasar emission lines of C III] and Mg II are weak or entirely absent. Detailed modeling of this spectrum will help elucidate fundamental questions regarding the nature of the emission processes at work in TDFs, while future UV spectroscopy of ASASSN-14li would help to confirm (or refute) the previously proposed connection between TDFs and "N-rich" quasars.
C1 [Cenko, S. Bradley; Cucchiara, Antonino; Pasham, Dheeraj R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley; Veilleux, Sylvain; Pasham, Dheeraj R.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Cucchiara, Antonino; Fruchter, Andrew S.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Roth, Nathaniel; Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Veilleux, Sylvain; Gezari, Suvi; Tombesi, Francesco] Univ Maryland, Dept Astron, Stadium Dr, College Pk, MD 20742 USA.
[Prochaska, J. Xavier; Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Guillochon, James] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Maksym, W. Peter] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Maksym, W. Peter] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Arcavi, Iair] Las Cumbres Observ Global Telescope, 6740 Cortona Dr,Suite 102, Goleta, CA 93111 USA.
[Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Butler, Nathaniel R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Filippenko, Alexei V.; Kasen, Daniel] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Nucl Sci, Berkeley, CA 94720 USA.
[Levan, Andrew J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Miller, Jon M.] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48103 USA.
[Strubbe, Linda E.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Strubbe, Linda E.] Univ British Columbia, Carl Wieman Sci Educ Initiat, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Tanvir, Nial R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Tombesi, Francesco] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Cenko, SB (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
EM brad.cenko@nasa.gov
OI Roth, Nathaniel/0000-0002-6485-2259; Maksym, Walter/0000-0002-2203-7889;
Guillochon, James/0000-0002-9809-8215
FU Aspen Center for Physics; NSF [1066293, AST-1211916]; TABASGO
Foundation; Christopher R. Redlich Fund; Association of Universities for
Research in Astronomy, Inc., under NASA [NAS 5-26555]
FX We thank R. Chornock, M. Eracleous, P. Hall, and C. Kochanek for
valuable discussions, and the HST staff for the prompt scheduling of
these ToO observations. S.B.C. acknowledges the Aspen Center for Physics
and NSF Grant #1066293 for hospitality. AVF's research was funded by NSF
grant AST-1211916, the TABASGO Foundation, and the Christopher R.
Redlich Fund.; Based on observations made with the NASA/ESA Hubble Space
Telescope, obtained from the Data Archive at the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555.
NR 50
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2016
VL 818
IS 2
AR L32
DI 10.3847/2041-8205/818/2/L32
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE2GK
UT WOS:000370444800011
ER
PT J
AU Aloiz, E
Douglas, JG
Nagel, A
AF Aloiz, Emily
Douglas, Janet G.
Nagel, Alexander
TI Painted plaster and glazed brick fragments from Achaemenid Pasargadae
and Persepolis, Iran
SO HERITAGE SCIENCE
LA English
DT Article
AB Background: Architectural fragments of decorated walls, floors, and columns excavated by Ernst Herzfeld (1879-1948) at the archaeological sites of Persepolis and Pasargadae in Iran are housed in the Freer Study Collection at the Freer Gallery of Art and Arthur M. Sackler Gallery (FSG), Smithsonian Institution in Washington, DC. Technical studies of these painted earthen plasters and glazed brick fragments were undertaken to enhance our knowledge of materials and technology of Achaemenid Persia between the late sixth and fourth centuries BCE. Initial analysis was done on the surface of the fragments using non-invasive X-ray fluorescence with a portable instrument. Polished cross-sections were used to examine the layering stratigraphy of paints and glazes, and to undertake compositional analysis using scanning electron microscopy with energy-dispersive X-ray spectroscopy.
Results: Up to five layers of paint are present on the Pasargadae plaster, constituting the remnants of a geometric design. The plasters were bound with clay tempered with an organic material that has long since degraded, leaving small voids throughout. Pigments identified include Egyptian blue, malachite green, red ocher, and cinnabar red. The floor fragments from Persepolis were finished with a lime plaster and two layers of hematite-rich paint. The brick fragments from Persepolis were found to be composed of high-silica material similar to faience, which were decorated with alkaline glazes, including a yellow glazed colored with lead antimonate, gray glaze colored with magnesium and iron, and green glazed colored with copper.
Conclusions: While the exact ages of the finishes are unknown, a similar technology was employed to decorate Achaemenid architecture in its principle Iranian cities. The variety of materials excavated by Herzfeld demonstrates the ability of Achaemenid artisans to work with multiple mediums to create a polychromatic finish including that of glazed tiles, earthen plaster tempered with gravel, earthen plaster tempered with organic matter, colored earths, pigmented paints and lime plasters. The layering of these materials can be seen and analyzed in cross-section although surface deterioration is often quite severe. The analysis of the compositional data on the architectural fragments inform their long-term preservation at the FSG as well as at the sites themselves.
C1 [Aloiz, Emily] John Milner Associates Preservat, 3200 Lee Hwy, Arlington, VA 22207 USA.
[Douglas, Janet G.] Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
[Nagel, Alexander] Smithsonian Inst, Natl Museum Nat Hist, 10th St & Constitut Ave, Washington, DC 20560 USA.
RP Aloiz, E (reprint author), John Milner Associates Preservat, 3200 Lee Hwy, Arlington, VA 22207 USA.
EM emilya@jmapreservation.com
NR 33
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U1 2
U2 2
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 2050-7445
J9 HERIT SCI
JI Herit. Sci.
PD FEB 19
PY 2016
VL 4
AR 3
DI 10.1186/s40494-016-0072-7
PG 10
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA DE2TH
UT WOS:000370479400001
ER
PT J
AU Lovchinsky, I
Sushkov, AO
Urbach, E
de Leon, NP
Choi, S
De Greve, K
Evans, R
Gertner, R
Bersin, E
Muller, C
McGuinness, L
Jelezko, F
Walsworth, RL
Park, H
Lukin, MD
AF Lovchinsky, I.
Sushkov, A. O.
Urbach, E.
de Leon, N. P.
Choi, S.
De Greve, K.
Evans, R.
Gertner, R.
Bersin, E.
Mueller, C.
McGuinness, L.
Jelezko, F.
Walsworth, R. L.
Park, H.
Lukin, M. D.
TI APPLIED PHYSICS Nuclear magnetic resonance detection and spectroscopy of
single proteins using quantum logic
SO SCIENCE
LA English
DT Article
ID SPIN; NANOSCALE; MICROSCOPY; RESOLUTION; READOUT
AB Nuclear magnetic resonance spectroscopy is a powerful tool for the structural analysis of organic compounds and biomolecules but typically requires macroscopic sample quantities. We use a sensor, which consists of two quantum bits corresponding to an electronic spin and an ancillary nuclear spin, to demonstrate room temperaturemagnetic resonance detection and spectroscopy of multiple nuclear species within individual ubiquitin proteins attached to the diamond surface. Using quantum logic to improve readout fidelity and a surface-treatment technique to extend the spin coherence time of shallow nitrogen-vacancy centers, we demonstrate magnetic field sensitivity sufficient to detect individual proton spins within 1 second of integration. This gain in sensitivity enables high-confidence detection of individual proteins and allows us to observe spectral features that reveal information about their chemical composition.
C1 [Lovchinsky, I.; Sushkov, A. O.; Urbach, E.; de Leon, N. P.; Choi, S.; De Greve, K.; Evans, R.; Bersin, E.; Walsworth, R. L.; Park, H.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Lovchinsky, I.; Sushkov, A. O.; Urbach, E.; de Leon, N. P.; Choi, S.; De Greve, K.; Evans, R.; Bersin, E.; Walsworth, R. L.; Park, H.; Lukin, M. D.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[Mueller, C.; McGuinness, L.; Jelezko, F.] Univ Ulm, Inst Quantum Opt, D-89081 Ulm, Germany.
[Mueller, C.; McGuinness, L.; Jelezko, F.] Univ Ulm, Ctr Integrated Quantum Sci & Technol IQST, D-89081 Ulm, Germany.
[Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Walsworth, R. L.; Park, H.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA.
[Park, H.] Broad Inst MIT & Harvard, Cambridge Ctr 7, Cambridge, MA 02142 USA.
[Sushkov, A. O.] Boston Univ, Dept Phys, 590 Commonwealth Ave, Boston, MA 02215 USA.
[de Leon, N. P.] Princeton Univ, Dept Elect Engn, Olden St, Princeton, NJ 08544 USA.
RP Park, H; Lukin, MD (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.; Park, H; Lukin, MD (reprint author), Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.; Park, H (reprint author), Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA.; Park, H (reprint author), Broad Inst MIT & Harvard, Cambridge Ctr 7, Cambridge, MA 02142 USA.
EM hongkun_park@harvard.edu; lukin@physics.harvard.edu
FU Defense Advanced Research Projects Agency (QuASAR program); NSF; Center
for Ultracold Atoms; Army Research Office Multidisciplinary University
Research Initiative; National Security Science and Engineering Faculty
Fellowship program,; Gordon and Betty Moore Foundation; Air Force Office
of Scientific Research National Defense Science and Engineering Graduate
Fellowship [32 CFR 168a]; European Research Council; German Academic
Exchange Service (DAAD) P.R.I.M.E. Fellowship; Herchel Smith-Harvard
Undergraduate Summer Research Program
FX We thank M. L. Pham, N. Chisholm, G. Kucsko, B. Harada, A. Ajoy, and P.
Cappellaro for helpful discussions and experimental help. This work was
supported by the Defense Advanced Research Projects Agency (QuASAR
program), NSF, the Center for Ultracold Atoms, the Army Research Office
Multidisciplinary University Research Initiative, the National Security
Science and Engineering Faculty Fellowship program, and the Gordon and
Betty Moore Foundation. I.L. was supported by the Air Force Office of
Scientific Research National Defense Science and Engineering Graduate
Fellowship (32 CFR 168a). Work at Ulm University was supported by the
European Research Council. L.M. acknowledges support by a German
Academic Exchange Service (DAAD) P.R.I.M.E. Fellowship. E.B. was
supported by the Herchel Smith-Harvard Undergraduate Summer Research
Program.
NR 29
TC 26
Z9 26
U1 21
U2 80
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD FEB 19
PY 2016
VL 351
IS 6275
BP 836
EP 841
DI 10.1126/science.aad8022
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DE0PB
UT WOS:000370325700039
PM 26847544
ER
PT J
AU Freeman, CJ
Stoner, EW
Easson, CG
Matterson, KO
Baker, DM
AF Freeman, Christopher J.
Stoner, Elizabeth W.
Easson, Cole G.
Matterson, Kenan O.
Baker, David M.
TI Symbiont carbon and nitrogen assimilation in the Cassiopea-Symbiodinium
mutualism
SO MARINE ECOLOGY PROGRESS SERIES
LA English
DT Article
DE Jellyfish; Symbiosis; Photosymbionts; Nutrient dynamics; Stable
isotopes; Carbon fixation; C-13 and N-15 tracers
ID JELLYFISH CASSIOPEA; DIVERSITY; XAMACHANA; PRODUCTIVITY; SPECIFICITY;
ABUNDANCE; EVOLUTION; SIZE; REEF
AB Symbiotic interactions in the marine environment have long been represented by mutualisms between photosymbionts and benthic marine invertebrates like corals and sponges. Although 'upside-down' epibenthic jellyfish in the genus Cassiopea also derive a substantial metabolic benefit from abundant communities of the dinoflagellate symbiont Symbiodinium, comparatively little is known about the efficiency of carbon (C) and nitrogen (N) assimilation within the Cassiopea holobiont. Using standardized 6 h incubations with C-13- and N-15-enriched compounds, we assessed symbiont C and N assimilation in both oral arm and bell tissue of C. xamachana under light and dark conditions. Carbon fixation was light dependent and highest in the photosymbiont-rich oral arm tissue. In contrast, (NO3)-N-15 assimilation was light independent in both tissue types and was highest in bell tissue that was sparsely colonized by photosymbionts. This, coupled with higher bell tissue N-15 enrichment under dark conditions, implicates non-photosynthetic microbes in Cassiopea N metabolism. This zonation of microbial activity may allow C. xamachana to simultaneously fix C and assimilate ambient or porewater N released during Cassiopea pumping activity. Although C. xamachana may utilize symbiont-derived N, lower N-15 enrichment relative to C fixation suggests that Cassiopea may also rely on exogenous sources of N for growth. This study provides initial evidence that the efficiency of symbiont metabolism within Cassiopea jellyfish is comparable to, or exceeds, that of other common benthic marine invertebrates, sup porting the contention that Cassiopea have an important role in the productivity and nutrient dynamics within their local environment.
C1 [Freeman, Christopher J.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
[Stoner, Elizabeth W.] Loxahatchee River Dist, 2500 Jupiter Pk Dr, Jupiter, FL 33458 USA.
[Easson, Cole G.; Matterson, Kenan O.] Univ Alabama Birmingham, Dept Biol, 1300 Univ Blvd, Birmingham, AL 35294 USA.
[Baker, David M.] Univ Hong Kong, Sch Biol Sci, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China.
[Baker, David M.] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China.
RP Freeman, CJ (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM freemanc@si.edu
FU Smithsonian Institution's Marine Global Earth Observatory (MarineGEO);
Tennenbaum Marine Observatories Network (TMON) initiatives
FX We thank R. Collin, G. Jacome, and P. Gondola at the Smithsonian
Tropical Research Institute in Bocas del Toro, Panama, for logistical
support. Financial support for this project came from a postdoctoral
fellowship awarded to C.J.F. from the Smithsonian Institution's Marine
Global Earth Observatory (MarineGEO) and Tennenbaum Marine Observatories
Network (TMON) initiatives. This is contribution number 1023 from the
Smithsonian Marine Station at Fort Pierce, Florida.
NR 25
TC 1
Z9 1
U1 11
U2 27
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0171-8630
EI 1616-1599
J9 MAR ECOL PROG SER
JI Mar. Ecol.-Prog. Ser.
PD FEB 18
PY 2016
VL 544
BP 281
EP 286
DI 10.3354/meps11605
PG 6
WC Ecology; Marine & Freshwater Biology; Oceanography
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Oceanography
GA DF2AW
UT WOS:000371142500020
ER
PT J
AU Savaris, M
Marinoni, L
Mathis, WN
AF Savaris, Marcoandre
Marinoni, Luciane
Mathis, Wayne N.
TI Revision of the shore-fly genus Peltopsilopa Hendel (Diptera:
Ephydridae)
SO ZOOTAXA
LA English
DT Article
DE Discomyzinae; Psilopini; taxonomy; systematics; New World
AB The Neotropical shore-fly genus Peltopsilopa Hendel is revised and now includes three species: P. acuta n.sp.; P. anisotomoides (Karsch), new combination; and P. schwarzi Cresson. A fourth species name, P. aspistes Hendel, is recognized as a junior synonym of P. anisotomoides (Karsch). We confirm that Peltopsilopa is closely related to Cressonomyia Arnaud and that the genus is in the tribe Psilopini, subfamily Discomyzinae. We provide a revised generic diagnosis and key to South American genera of Psilopini to facilitate identification of Peltopsilopa. The included species descriptions are extensively documented with illustrations, photographs, and distribution map.
C1 [Savaris, Marcoandre; Marinoni, Luciane] Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil.
[Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA.
RP Savaris, M; Marinoni, L (reprint author), Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil.; Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA.
EM plaumannimyia@gmail.com; lmarinoni@ufpr.br; mathisw@si.edu
RI Marinoni, Luciane /C-5720-2013
FU CNPq [200277/2015-4]
FX We thank Allen L. Norrbom (USDA, Systematic Entomology Laboratory),
Daniel Negoseki Robalo Costa, Tadeusz Zatwarnicki, Mercedes Lizarralde
de Grosso, and an anonymous reviewer for their reviews of the
manuscript. Tadeusz Zatwarnicki provided the initial information on the
female syntype of Celyphus anisotomoides Karsch (ZMHU) and informed us
that this syntype is a species in the genus Peltopsilopa. We are
especially grateful to the curators listed previously who sent specimens
or photographs. Their invaluable assistance made this paper possible. We
thank CNPq for financial support for this study (Process number
200277/2015-4).
NR 17
TC 1
Z9 1
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 18
PY 2016
VL 4083
IS 1
BP 83
EP 98
PG 16
WC Zoology
SC Zoology
GA DF4SZ
UT WOS:000371342300004
PM 27394220
ER
PT J
AU Kelez, S
Velez-Zuazo, X
Pacheco, AS
AF Kelez, Shaleyla
Velez-Zuazo, Ximena
Pacheco, Aldo S.
TI First record of hybridization between green Chelonia mydas and hawksbill
Eretmochelys imbricata sea turtles in the Southeast Pacific
SO PEERJ
LA English
DT Article
DE Hybridization; Cheloniidae; Interspecific breeding; Cytochrome oxidase
I; Female Eretmochelys imbricata
AB Hybridization among sea turtle species has been widely reported in the Atlantic Ocean, but their detection in the Pacific Ocean is limited to just two individual hybrid turtles, in the northern hemisphere. Herein, we report, for the first time in the southeast Pacific, the presence of a sea turtle hybrid between the green turtle Chelonia mydas and the hawksbill turtle Eretmochelys imbricata. This juvenile sea turtle was captured in northern Peru (4 degrees 13'S; 81 degrees 10'W) on the 5(th) of January, 2014. The individual exhibited morphological characteristics of C. mydas such as dark green coloration, single pair of pre-frontal scales, four post-orbital scales, and mandibular median ridge, while the presence of two claws in each frontal flipper, and elongated snout resembled the features of E. imbricata. In addition to morphological evidence, we confirmed the hybrid status of this animal using genetic analysis of the mitochondrial gene cytochrome oxidase I, which revealed that the hybrid individual resulted from the cross between a female E. imbricata and a male C. mydas. Our report extends the geographical range of occurrence of hybrid sea turtles in the Pacific Ocean, and is a significant observation of interspecific breeding between one of the world's most critically endangered populations of sea turtles, the east Pacific E. imbricata, and a relatively healthy population, the east Pacific C. mydas.
C1 [Kelez, Shaleyla; Velez-Zuazo, Ximena; Pacheco, Aldo S.] EcOceanica, Lima, Peru.
[Velez-Zuazo, Ximena] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Sustainabil, Washington, DC 20008 USA.
[Pacheco, Aldo S.] Univ Antofagasta, Fac Ciencias Mar & Recursos Biol, Inst Ciencias Nat Alexander von Humboldt, Antofagasta, Chile.
RP Kelez, S (reprint author), EcOceanica, Lima, Peru.
EM shaleyla.kelez@ecoceanica.org
FU Duke Marine Laboratory; Fund for Nature-Japan; Principia College; Krilca
Gifts; CNPC-Peru; ecOceanica turtle adoption program
FX Duke Marine Laboratory, Fund for Nature-Japan, Principia College, Krilca
Gifts, CNPC-Peru and ecOceanica turtle adoption program provided funds
for our research in northern Peru. The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 22
TC 1
Z9 1
U1 8
U2 15
PU PEERJ INC
PI LONDON
PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND
SN 2167-8359
J9 PEERJ
JI PeerJ
PD FEB 18
PY 2016
VL 4
AR e1712
DI 10.7717/peerj.1712
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DE9UF
UT WOS:000370984200009
PM 26925333
ER
PT J
AU Patla, BR
AF Patla, B. R.
TI Reduction of magnetic perturbation for SR-POEM
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE weak equivalence principle; magnetic fields; tests of general relativity
ID ACCURACY EVALUATION; COMPENSATION; SHIELDS; FIELD
AB SR-POEM is a Galilean test of the weak equivalence principle that aims to measure the fractional acceleration difference. with a mission uncertainty sigma(eta) = 1 x 10(-17) for a pair of test substances. It is to be conducted during the low-drag free fall portion of a sounding rocket flight. The interaction of the magnetic field gradient with tiny remanent magnetic moments of the test masses will produce a spurious acceleration that is not sufficiently reduced by a single Mu-metal shield. In this paper, we study configurations with two and three shields. Approximate analytic formulae are used to study the shielding factor as a function of geometry. We use finite element analysis (FEA) to determine the magnetic field and gradient for certain cases that satisfy the mission requirements. FEA results are compared with analytic expressions wherever appropriate. Several configurations reduce both axial and transverse magnetic field within the shielding volume by at least the required factor of 4 x 10(5).
C1 [Patla, B. R.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Patla, B. R.] Natl Inst Stand & Technol, 325 Broadway St, Boulder, CO 80305 USA.
RP Patla, BR (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Patla, BR (reprint author), Natl Inst Stand & Technol, 325 Broadway St, Boulder, CO 80305 USA.
EM bijunath.patla@nist.gov
FU NASA [NNX08AO04G]; NASA, Division of Planetary Science [NNH12AT81I]
FX This work was supported by NASA grant NNX08AO04G. We thank Robert
Reasenberg and James Phillips for their help in getting this work
started and for their guidance and suggestions as the manuscript
evolved. We also thank Neil Ashby, Stephan Barlow, Jens Gundlach, Tom
Heavner, Mauro Hueller, Steven Jefferts, John Mester, Riley Newman,
Vishal Shah and Tim Sumner for useful discussions. We would like to
extend our thanks to two anonymous referees for their valuable
suggestions that have helped improve this paper. This work was also
supported in part by NASA, Division of Planetary Science, under grant
NNH12AT81I.
NR 29
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD FEB 18
PY 2016
VL 33
IS 4
AR 045006
DI 10.1088/0264-9381/33/4/045006
PG 17
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA DC2NP
UT WOS:000369053700007
ER
PT J
AU Aguila, RN
Davis, DR
AF Aguila, Rayner Nunez
Davis, Don R.
TI Antillonatus, a new replacement name for the generic homonym
Antillopsyche Nunez & Davis, 2016 (Lepidoptera: Tineoidea: Psychidae)
SO ZOOTAXA
LA English
DT Letter
C1 [Aguila, Rayner Nunez] Bavarian State Collect Zool, Sect Lepidoptera, Munich, Germany.
[Davis, Don R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
RP Aguila, RN (reprint author), Bavarian State Collect Zool, Sect Lepidoptera, Munich, Germany.
EM raynernunez75@gmail.com; davisd@si.edu
NR 2
TC 0
Z9 0
U1 1
U2 2
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 16
PY 2016
VL 4079
IS 5
BP 595
EP 595
PG 1
WC Zoology
SC Zoology
GA DD7UN
UT WOS:000370130300006
PM 27394211
ER
PT J
AU Holmquist, JR
Booth, RK
MacDonald, GM
AF Holmquist, James R.
Booth, Robert K.
MacDonald, Glen M.
TI Boreal peatland water table depth and carbon accumulation during the
Holocene thermal maximum, Roman Warm Period, and Medieval Climate
Anomaly
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Testate Amoebae; Peatlands; Boreal; James Bay Lowland; Holocene Thermal
Maximum; Medieval Climate Anomaly; Roman Warm Period
ID HUDSON-BAY LOWLANDS; NORTHERN GREAT-PLAINS; SUB-ARCTIC QUEBEC;
LAKE-LEVEL CHANGE; ROCKY-MOUNTAINS; TESTATE AMEBAS; UNITED-STATES;
HYDROLOGIC VARIABILITY; ENVIRONMENTAL-CHANGES; PAST MILLENNIUM
AB The Boreal Shield and James Bay Lowland regions of Ontario have few Holocene reconstructions specific to surface moisture despite their potential importance to documenting the geographic patterns and teleconnections of Holocene pluvials and droughts, as well as their role in the global carbon cycle. We reconstructed water table depth using preserved testate amoebae in four stratigraphic peatland cores, supplemented with a literature review to investigate the effects of the Holocene Thermal Maximum (HTM) and Medieval Climate Anomaly (MCA) on surface moisture and long-term apparent carbon accumulation (LARCA) in the regions. A 7320 calendar years before AD 1950 (yrBP) length record registered a wet shift at 4600 yrBP in concert with the HTM and a later post-2550 yrBP shift towards wetter and more stable conditions, possibly related to the Roman Warm Period. During the late-Holocene the three most southern boreal records indicated a lack of droughts during the MCA. Medieval pluvials in boreal Ontario would be consistent with North American precipitation patterns under La Nifia conditions. Of the three wet-warm periods identified (HTM, 2550 yrBP, MCA), the 2550 yrBP shift had the most consistent positive influence on LARCA regionally. Although past precipitation was positively correlated with temperature in the region, recent drying may be indicative of a fundamental change in evaporation-precipitation balance. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Holmquist, James R.] Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
[Booth, Robert K.] Lehigh Univ, Earth & Environm Sci Dept, Bethlehem, PA USA.
[MacDonald, Glen M.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
RP Holmquist, JR (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM HolmquistJ@si.edu
RI Booth, Robert/G-5563-2010
FU National Science Foundation [NSF 0843685, NSF-0628598]
FX This research was made possible by grants from the National Science
Foundation (NSF 0843685; NSF-0628598). The authors thank David Beilman
for collaboration on the 2008 fieldwork and Konstantine Kreminitsky,
Nicolai Kondov, Karly Wagner, Alvin Li, Julianne Lee, Michelle Lim, and
Loren Quintana for laboratory assistance. The authors also thank two
anonymous reviewers for their contributions towards improving this
manuscript.
NR 103
TC 1
Z9 1
U1 11
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD FEB 15
PY 2016
VL 444
BP 15
EP 27
DI 10.1016/j.palaeo.2015.11.035
PG 13
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA DD7HA
UT WOS:000370093100002
ER
PT J
AU Krawczynski, HS
Stern, D
Harrison, FA
Kislat, FF
Zajczyk, A
Beilicke, M
Hoormann, J
Guo, Q
Endsley, R
Ingram, AR
Miyasaka, H
Madsen, KK
Aaron, KM
Amini, R
Baring, MG
Beheshtipour, B
Bodaghee, A
Booth, J
Borden, C
Bottcher, M
Christensen, FE
Coppi, PS
Cowsik, R
Davis, S
Dexter, J
Done, C
Dominguez, LA
Ellison, D
English, RJ
Fabian, AC
Falcone, A
Favretto, JA
Fernandez, R
Giommi, P
Grefenstette, BW
Kara, E
Lee, CH
Lyutikov, M
Maccarone, T
Matsumoto, H
McKinney, J
Mihara, T
Miller, JM
Narayan, R
Natalucci, L
Ozel, F
Pivovaroff, MJ
Pravdo, S
Psaltis, D
Okajima, T
Toma, K
Zhang, WW
AF Krawczynski, Henric S.
Stern, Daniel
Harrison, Fiona A.
Kislat, Fabian F.
Zajczyk, Anna
Beilicke, Matthias
Hoormann, Janie
Guo, Qingzhen
Endsley, Ryan
Ingram, Adam R.
Miyasaka, Hiromasa
Madsen, Kristin K.
Aaron, Kim M.
Amini, Rashied
Baring, Matthew G.
Beheshtipour, Banafsheh
Bodaghee, Arash
Booth, Jeffrey
Borden, Chester
Boettcher, Markus
Christensen, Finn E.
Coppi, Paolo S.
Cowsik, Ramanath
Davis, Shane
Dexter, Jason
Done, Chris
Dominguez, Luis A.
Ellison, Don
English, Robin J.
Fabian, Andrew C.
Falcone, Abe
Favretto, Jeffrey A.
Fernandez, Rodrigo
Giommi, Paolo
Grefenstette, Brian W.
Kara, Erin
Lee, Chung H.
Lyutikov, Maxim
Maccarone, Thomas
Matsumoto, Hironori
McKinney, Jonathan
Mihara, Tatehiro
Miller, Jon M.
Narayan, Ramesh
Natalucci, Lorenzo
Oezel, Feryal
Pivovaroff, Michael J.
Pravdo, Steven
Psaltis, Dimitrios
Okajima, Takashi
Toma, Kenji
Zhang, William W.
TI X-ray polarimetry with the Polarization Spectroscopic Telescope Array
(PolSTAR)
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE X-ray polarimetry; Astronomical instrumentation; Black holes; Neutron
stars; Blazars; General relativity
ID ACCRETING BLACK-HOLES; MAGNETIZED NEUTRON-STARS; GENERAL-RELATIVISTIC
MAGNETOHYDRODYNAMICS; QUASI-PERIODIC OSCILLATIONS; SUPER-EDDINGTON
ACCRETION; ACTIVE GALACTIC NUCLEI; CRAB-NEBULA; CYGNUS X-1; CYCLOTRON
LINE; NUSTAR DISCOVERY
AB This paper describes the Polarization Spectroscopic Telescope Array (PolSTAR), a mission proposed to NASA's 2014 Small Explorer (SMEX) announcement of opportunity. PolSTAR measures the linear polarization of 3-50 keV (requirement; goal: 2.5-70 keV) X-rays probing the behavior of matter, radiation and the very fabric of spacetime under the extreme conditions close to the event horizons of black holes, as well as in and around magnetars and neutron stars. The PolSTAR design is based on the technology developed for the Nuclear Spectroscopic Telescope Array (NuSTAR) mission launched in June 2012. In particular, it uses the same X-ray optics, extendable telescope boom, optical bench, and CdZnTe detectors as NuSTAR. The mission has the sensitivity to measure similar to 1% linear polarization fractions for X-ray sources with fluxes down to similar to 5 mCrab. This paper describes the PolSTAR design as well as the science drivers and the potential science return. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Krawczynski, Henric S.; Kislat, Fabian F.; Zajczyk, Anna; Beilicke, Matthias; Hoormann, Janie; Guo, Qingzhen; Endsley, Ryan; Amini, Rashied; Beheshtipour, Banafsheh; Cowsik, Ramanath; Falcone, Abe] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Krawczynski, Henric S.; Kislat, Fabian F.; Zajczyk, Anna; Beilicke, Matthias; Hoormann, Janie; Guo, Qingzhen; Endsley, Ryan; Amini, Rashied; Beheshtipour, Banafsheh; Cowsik, Ramanath] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Stern, Daniel; Aaron, Kim M.; Amini, Rashied; Booth, Jeffrey; Borden, Chester; Dominguez, Luis A.; English, Robin J.; Falcone, Abe; Favretto, Jeffrey A.; Lee, Chung H.; Pravdo, Steven] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Harrison, Fiona A.; Miyasaka, Hiromasa; Madsen, Kristin K.; Grefenstette, Brian W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Ingram, Adam R.] Astron Inst Anton Pannekoek, Sci Pk 904,POB 94249, NL-1090 GE Amsterdam, Netherlands.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, POB 1892, Houston, TX 77251 USA.
[Bodaghee, Arash] Georgia Coll, Dept Chem Phys & Astron, Milledgeville, GA 31061 USA.
[Boettcher, Markus] North West Univ, Ctr Space Res, Private Bag X6001, ZA-2520 Potchefstroom, South Africa.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Coppi, Paolo S.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
[Davis, Shane] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[Dexter, Jason] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Done, Chris] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Ellison, Don] N Carolina State Univ, Dept Phys, 400L Riddick Hall, Raleigh, NC 27695 USA.
[Fabian, Andrew C.; Kara, Erin] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Falcone, Abe] Penn State Univ, Dept Astron & Astrophys, 516 Davey Lab, University Pk, PA 16802 USA.
[Fernandez, Rodrigo] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Fernandez, Rodrigo] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fernandez, Rodrigo] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[Giommi, Paolo] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy.
[Lyutikov, Maxim] Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
[Maccarone, Thomas] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA.
[Matsumoto, Hironori] Nagoya Univ, Ctr Expt Studies, Kobayashi Maskawa Inst Origin Particles & Univers, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
[McKinney, Jonathan] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Mihara, Tatehiro] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
[Miller, Jon M.] Univ Michigan, Dept Astron, 830 Dennison,500 Church St, Ann Arbor, MI 48109 USA.
[Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
[Natalucci, Lorenzo] INAF, Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
[Oezel, Feryal; Psaltis, Dimitrios] Univ Arizona, Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Okajima, Takashi; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Toma, Kenji] Tohoku Univ, Astron Inst, Aoba Ku, 6-3 Aramaki, Sendai, Miyagi 9808578, Japan.
RP Krawczynski, HS (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.; Krawczynski, HS (reprint author), Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
EM krawcz@wustl.edu
RI done, chris/D-4605-2016; Mihara, Tatehiro/C-5536-2017;
OI done, chris/0000-0002-1065-7239; Mihara, Tatehiro/0000-0002-6337-7943;
Narayan, Ramesh/0000-0002-1919-2730
FU McDonnell Center for the Space Sciences at Washington University; NASA
[NNX14AD19G, NNX13AQ82G, NNX13AP08G]; STFC [ST/L00075X/1]; NASA/NSF/TCAN
[NNX14AB46G]; NSF/XSEDE/TACC [TGPHY120005]; NASA/Pleiades [SMD-14-5451];
Netherlands Organization for Scientific Research (NWO) Veni Fellowship
[639.041.437]; University of California Office of the President; NSF
[AST-1206097]
FX HK thanks the McDonnell Center for the Space Sciences at Washington
University for sponsoring the design and fabrication of the X-Calibur
prototype polarimeter, and NASA Grant #NNX14AD19G for the support of the
X-Calibur balloon project. MGB acknowledges NASA Grants NNX13AQ82G and
NNX13AP08G for support. CD acknowledges STFC support from Grant
ST/L00075X/1. JCM acknowledges NASA/NSF/TCAN Grant NNX14AB46G,
NSF/XSEDE/TACC (TGPHY120005), and NASA/Pleiades (SMD-14-5451). Adam
Ingram (AI) grant no. 639.041.437 acknowledges support from the
Netherlands Organization for Scientific Research (NWO) Veni Fellowship.
RF acknowledges support from the University of California Office of the
President, and from NSF Grant AST-1206097.
NR 179
TC 2
Z9 2
U1 3
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD FEB 15
PY 2016
VL 75
BP 8
EP 28
DI 10.1016/j.astropartphys.2015.10.009
PG 21
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DC4SE
UT WOS:000369209800002
ER
PT J
AU Schmidt, R
Lemeshko, M
AF Schmidt, Richard
Lemeshko, Mikhail
TI Deformation of a Quantum Many-Particle System by a Rotating Impurity
SO PHYSICAL REVIEW X
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATE; RANGE RYDBERG MOLECULES; ULTRACOLD MOLECULES;
SUPERFLUID; HELIUM; SCATTERING; POLARONS
AB During the past 70 years, the quantum theory of angular momentum has been successfully applied to describing the properties of nuclei, atoms, and molecules, and their interactions with each other as well as with external fields. Because of the properties of quantum rotations, the angular-momentum algebra can be of tremendous complexity even for a few interacting particles, such as valence electrons of an atom, not to mention larger many-particle systems. In this work, we study an example of the latter: a rotating quantum impurity coupled to a many-body bosonic bath. In the regime of strong impurity-bath couplings, the problem involves the addition of an infinite number of angular momenta, which renders it intractable using currently available techniques. Here, we introduce a novel canonical transformation that allows us to eliminate the complex angular-momentum algebra from such a class of many-body problems. In addition, the transformation exposes the problem's constants of motion, and renders it solvable exactly in the limit of a slowly rotating impurity. We exemplify the technique by showing that there exists a critical rotational speed at which the impurity suddenly acquires one quantum of angular momentum from the many-particle bath. Such an instability is accompanied by the deformation of the phonon density in the frame rotating along with the impurity.
C1 [Schmidt, Richard] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Schmidt, Richard] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Lemeshko, Mikhail] IST Austria, A-3400 Klosterneuburg, Austria.
RP Lemeshko, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
EM richard.schmidt@cfa.harvard.edu; mikhail.lemeshko@ist.ac.at
FU NSF
FX We are grateful to Eugene Demler, Jan Kaczmarczyk, Laleh Safari, and
Hendrik Weimer for insightful discussions. The work was supported by the
NSF through a grant for the Institute for Theoretical Atomic, Molecular,
and Optical Physics at Harvard University and Smithsonian Astrophysical
Observatory.
NR 53
TC 7
Z9 7
U1 3
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2160-3308
J9 PHYS REV X
JI Phys. Rev. X
PD FEB 12
PY 2016
VL 6
IS 1
AR 011012
DI 10.1103/PhysRevX.6.011012
PG 13
WC Physics, Multidisciplinary
SC Physics
GA DD6JF
UT WOS:000370029800001
ER
PT J
AU Pinault, L
Tjepkema, M
Crouse, DL
Weichenthal, S
van Donkelaar, A
Martin, RV
Brauer, M
Chen, H
Burnett, RT
AF Pinault, Lauren
Tjepkema, Michael
Crouse, Daniel L.
Weichenthal, Scott
van Donkelaar, Aaron
Martin, Randall V.
Brauer, Michael
Chen, Hong
Burnett, Richard T.
TI Risk estimates of mortality attributed to low concentrations of ambient
fine particulate matter in the Canadian community health survey cohort
SO ENVIRONMENTAL HEALTH
LA English
DT Article
DE PM2.5; Fine particulate matter; Air pollution; Cardiovascular mortality;
Respiratory mortality
ID LONG-TERM EXPOSURE; CORONARY-HEART-DISEASE; AIR-POLLUTION; FOLLOW-UP;
MILLION ADULTS; ASSOCIATIONS
AB Background: Understanding the shape of the relationship between long-term exposure to ambient fine particulate matter (PM2.5) concentrations and health risks is critical for health impact and risk assessment. Studies evaluating the health risks of exposure to low concentrations of PM2.5 are limited. Further, many existing studies lack individual-level information on potentially important behavioural confounding factors.
Methods: A prospective cohort study was conducted among a subset of participants in a cohort that linked respondents of the Canadian Community Health Survey to mortality (n = 299,500) with satellite-derived ambient PM2.5 estimates. Participants enrolled between 2000 and 2008 were followed to date of death or December 31, 2011. Cox proportional hazards models were used to estimate hazard ratios (HRs) for mortality attributed to PM2.5 exposure, adjusted for individual-level and contextual covariates, including smoking behaviour and body mass index (BMI).
Results: Approximately 26,300 non-accidental deaths, of which 32.5 % were due to circulatory disease and 9.1 % were due to respiratory disease, occurred during the follow-up period. Ambient PM2.5 exposures were relatively low (mean = 6.3 mu g/m(3)), yet each 10 mu g/m(3) increase in exposure was associated with increased risks of non-accidental (HR = 1.26; 95 % CI: 1.19-1.34), circulatory disease (HR = 1.19; 95 % CI: 1.07-1.31), and respiratory disease mortality (HR = 1.52; 95 % CI: 1.26-1.84) in fully adjusted models. Higher hazard ratios were observed for respiratory mortality among respondents who never smoked (HR = 1.97; 95 % CI: 1.24-3.13 vs. HR = 1.45; 95 % CI: 1.17-1.79 for ever smokers), and among obese (BMI = 30) respondents (HR = 1.76; 95 % CI: 1.15-2.69 vs. HR = 1.41; 95 % CI: 1.04-1.91 for normal weight respondents), though differences between groups were not statistically significant. A threshold analysis for non-accidental mortality estimated a threshold concentration of 0 mu g/m(3) (+95 % CI = 4.5 mu g/m(3)).
Conclusions: Increased risks of non-accidental, circulatory, and respiratory mortality were observed even at very low concentrations of ambient PM2.5. HRs were generally greater than most literature values, and adjusting for behavioural covariates served to reduce HR estimates slightly.
C1 [Pinault, Lauren; Tjepkema, Michael] STAT Canada, Hlth Anal Div, 100 Tunneys Pasture Driveway, Ottawa, ON K1A 0T6, Canada.
[Crouse, Daniel L.] Univ New Brunswick, NB IRDT, POB 4400, Fredericton, NB E3B 5A3, Canada.
[Crouse, Daniel L.] Univ New Brunswick, Dept Sociol, POB 4400, Fredericton, NB E3B 5A3, Canada.
[Weichenthal, Scott] Hlth Canada, Air Hlth Effects Sci Div, 269 Laurier Ave West, Ottawa, ON K1A 0K9, Canada.
[van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, 6310 Coburg Rd, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Brauer, Michael] Univ British Columbia, Fac Med, Sch Populat & Publ Hlth, 2206 East Mall, Vancouver, BC V6T 1Z3, Canada.
[Chen, Hong] Publ Hlth Ontario, Suite 300,480 Univ Ave, Toronto, ON M5G 1V2, Canada.
[Burnett, Richard T.] Hlth Canada, Environm Hlth Sci & Res Bur, 50 Columbine Driveway, Ottawa, ON K1A 0L2, Canada.
RP Pinault, L (reprint author), STAT Canada, Hlth Anal Div, 100 Tunneys Pasture Driveway, Ottawa, ON K1A 0T6, Canada.
EM Lauren.Pinault@canada.ca
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
NR 36
TC 1
Z9 1
U1 2
U2 13
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1476-069X
J9 ENVIRON HEALTH-GLOB
JI Environ. Health
PD FEB 11
PY 2016
VL 15
AR 18
DI 10.1186/s12940-016-0111-6
PG 15
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA DE2TC
UT WOS:000370478900003
PM 26864652
ER
PT J
AU Huang, YM
Rueda, LM
AF Huang, Yiau-Min
Rueda, Leopoldo M.
TI A pictorial key to the sections, groups, and species of the Aedes
(Diceromyia) in the Afrotropical Region (Diptera: Culicidae)
SO ZOOTAXA
LA English
DT Article
DE Culicidae; mosquitoes; identification key; Aedes; Africa
ID YELLOW-FEVER VIRUS; SOUTHEASTERN SENEGAL; CHIKUNGUNYA OUTBREAK; SOUTHERN
RHODESIA; FURCIFER-TAYLORI; MOSQUITOS; DENGUE-2; EPIDEMIC
AB Nine species of the subgenus Diceromyia Theobald of genus Aedes Meigen in the Afrotropical Region are treated in a pictorial key based on diagnostic morphological features. Images of the diagnostic morphological structures of the adult head, thorax, abdomen, leg and wing are included. The medical importance of the Furcifer Group species in Africa was briefly reviewed.
C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA.
[Rueda, Leopoldo M.] Walter Reed Army Inst Res, Entomol Branch, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA.
[Rueda, Leopoldo M.] Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA.
RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA.; Rueda, LM (reprint author), Walter Reed Army Inst Res, Entomol Branch, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA.; Rueda, LM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM huangy@si.edu; ruedapol@si.edu
NR 35
TC 0
Z9 0
U1 0
U2 3
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 11
PY 2016
VL 4079
IS 2
BP 281
EP 290
PG 10
WC Zoology
SC Zoology
GA DD7UC
UT WOS:000370128900009
PM 27396006
ER
PT J
AU Poorter, L
Ongers, FB
Aide, TM
Zambrano, AMA
Balvanera, P
Becknell, JM
Boukili, V
Brancalion, PHS
Broadbent, EN
Chazdon, RL
Craven, D
de Almeida-Cortez, JS
Cabral, GAL
de Jong, BHJ
Denslow, JS
Dent, DH
DeWalt, SJ
Dupuy, JM
Duran, SM
Espirito-Santo, MM
Fandino, MC
Cesar, RG
Hall, JS
Hernandez-Stefanoni, JL
Jakovac, CC
Junqueira, AB
Kennard, D
Letcher, SG
Licona, JC
Lohbeck, M
Marin-Spiotta, E
Martinez-Ramos, M
Massoca, P
Meave, JA
Mesquita, R
Mora, F
Munoz, R
Muscarella, R
Nunes, YRF
Ochoa-Gaona, S
de Oliveira, AA
Orihuela-Belmonte, E
Pena-Claros, M
Perez-Garcia, EA
Piotto, D
Powers, JS
Rodriguez-Velazquez, J
Romero-Perez, IE
Ruiz, J
Saldarriaga, JG
Sanchez-Azofeifa, A
Schwartz, NB
Steininger, MK
Swenson, NG
Toledo, M
Uriarte, M
van Breugel, M
van der Wal, H
Veloso, MDM
Vester, HFM
Vicentini, A
Vieira, ICG
Bentos, TV
Williamson, GB
Rozendaal, DMA
AF Poorter, Lourens
Ongers, Frans B.
Aide, T. Mitchell
Zambrano, Angelica M. Almeyda
Balvanera, Patricia
Becknell, Justin M.
Boukili, Vanessa
Brancalion, Pedro H. S.
Broadbent, Eben N.
Chazdon, Robin L.
Craven, Dylan
de Almeida-Cortez, Jarcilene S.
Cabral, George A. L.
de Jong, Ben H. J.
Denslow, Julie S.
Dent, Daisy H.
DeWalt, Saara J.
Dupuy, Juan M.
Duran, Sandra M.
Espirito-Santo, Mario M.
Fandino, Maria C.
Cesar, Ricardo G.
Hall, Jefferson S.
Hernandez-Stefanoni, Jose Luis
Jakovac, Catarina C.
Junqueira, Andre B.
Kennard, Deborah
Letcher, Susan G.
Licona, Juan-Carlos
Lohbeck, Madelon
Marin-Spiotta, Erika
Martinez-Ramos, Miguel
Massoca, Paulo
Meave, Jorge A.
Mesquita, Rita
Mora, Francisco
Munoz, Rodrigo
Muscarella, Robert
Nunes, Yule R. F.
Ochoa-Gaona, Susana
de Oliveira, Alexandre A. .
Orihuela-Belmonte, Edith
Pena-Claros, Marielos
Perez-Garcia, Eduardo A. .
Piotto, Daniel
Powers, Jennifer S.
Rodriguez-Velazquez, Jorge
Romero-Perez, I. Eunice
Ruiz, Jorge
Saldarriaga, Juan G.
Sanchez-Azofeifa, Arturo
Schwartz, Naomi B.
Steininger, Marc K.
Swenson, Nathan G.
Toledo, Marisol
Uriarte, Maria
van Breugel, Michiel
van der Wal, Hans
Veloso, Maria D. M.
Vester, Hans F. M.
Vicentini, Alberto
Vieira, Ima C. G.
Bentos, Tony Vizcarra
Williamson, G. Bruce
Rozendaal, Danae M. A.
TI Biomass resilience of Neotropical secondary forests
SO NATURE
LA English
DT Article
ID TROPICAL DRY FOREST; NORTHEASTERN COSTA-RICA; ABOVEGROUND BIOMASS;
CARBON STOCKS; SPECIES COMPOSITION; ECOSYSTEM SERVICES; AMAZONIAN
FORESTS; RAIN-FORESTS; STAND AGE; LAND-USE
AB Land-use change occurs nowhere more rapidly than in the tropics, where the imbalance between deforestation and forest regrowth has large consequences for the global carbon cycle(1). However, considerable uncertainty remains about the rate of biomass recovery in secondary forests, and how these rates are influenced by climate, landscape, and prior land use(2-4). Here we analyse aboveground biomass recovery during secondary succession in 45 forest sites and about 1,500 forest plots covering the major environmental gradients in the Neotropics. The studied secondary forests are highly productive and resilient. Aboveground biomass recovery after 20 years was on average 122 megagrams per hectare (Mg ha(-1)), corresponding to a net carbon uptake of 3.05 Mg C ha(-1) yr(-1), 11 times the uptake rate of old-growth forests. Aboveground biomass stocks took a median time of 66 years to recover to 90% of old-growth values. Aboveground biomass recovery after 20 years varied 11.3-fold ( from 20 to 225 Mg ha(-1)) across sites, and this recovery increased with water availability (higher local rainfall and lower climatic water deficit). We present a biomass recovery map of Latin America, which illustrates geographical and climatic variation in carbon sequestration potential during forest regrowth. The map will support policies to minimize forest loss in areas where biomass resilience is naturally low (such as seasonally dry forest regions) and promote forest regeneration and restoration in humid tropical lowland areas with high biomass resilience.
C1 [Poorter, Lourens; Ongers, Frans B.; Jakovac, Catarina C.; Lohbeck, Madelon; Pena-Claros, Marielos] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands.
[Aide, T. Mitchell] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA.
[Zambrano, Angelica M. Almeyda; Broadbent, Eben N.] Univ Alabama, Dept Geog, Spatial Ecol & Conservat Lab, Tuscaloosa, AL 35487 USA.
[Balvanera, Patricia; Martinez-Ramos, Miguel; Mora, Francisco; Rodriguez-Velazquez, Jorge] Univ Nacl Autonoma Mexico, Inst Invest Ecosistemas & Sustentabilidad, Morelia, Michoacan, Mexico.
[Becknell, Justin M.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
[Boukili, Vanessa; Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.
[Brancalion, Pedro H. S.; Cesar, Ricardo G.] Univ Sao Paulo, Luiz Queiroz Coll Agr, Dept Forest Sci, BR-13418900 Piracicaba, SP, Brazil.
[Craven, Dylan; Hall, Jefferson S.; van Breugel, Michiel] Smithsonian Trop Res Inst, SI ForestGEO, Balboa, Panama.
[Craven, Dylan] German Ctr Integrat Biodiversity Res iDiv Halle J, D-04103 Leipzig, Germany.
[Craven, Dylan] Univ Leipzig, Inst Biol, D-04103 Leipzig, Germany.
[de Almeida-Cortez, Jarcilene S.; Cabral, George A. L.] Univ Fed Pernambuco, Dept Bot, BR-50670901 Recife, PE, Brazil.
[de Jong, Ben H. J.; Ochoa-Gaona, Susana; Orihuela-Belmonte, Edith] El Colegio Frontera Sur, Unidad Campeche, Dept Sustainabil Sci, Campeche, Mexico.
[Denslow, Julie S.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70130 USA.
[Dent, Daisy H.] Smithsonian Trop Res Inst, Balboa, Panama.
[Dent, Daisy H.] Univ Stirling, Biol & Environm Sci, Stirling FK9 4LA, Scotland.
[DeWalt, Saara J.; Rozendaal, Danae M. A.] Clemson Univ, Dept Sci Biol, Clemson, SC 29634 USA.
[Dupuy, Juan M.; Hernandez-Stefanoni, Jose Luis] Ctr Invest Cient Yucatan, Unidad Recursos Nat, Merida, Yucatan, Mexico.
[Duran, Sandra M.; Sanchez-Azofeifa, Arturo] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Espirito-Santo, Mario M.; Nunes, Yule R. F.; Veloso, Maria D. M.] Univ Estadual Montes Claros, Dept Biol Geral, BR-39401089 Montes Claros, MG, Brazil.
[Fandino, Maria C.] Fondo Patrimonio Nat Biodiversidad & Areas Proteg, Bogota, Colombia.
[Jakovac, Catarina C.; Massoca, Paulo; Mesquita, Rita; Vicentini, Alberto; Bentos, Tony Vizcarra; Williamson, G. Bruce] Inst Nacl de Pesquisas da Amazonia, Environm Dynam Res Coordinat, Biol Dynam Forest Fragments Project, BR-69067375 Manaus, Amazonas, Brazil.
[Junqueira, Andre B.] Wageningen Univ, Ctr Crop Syst Anal, NL-6700 AK Wageningen, Netherlands.
[Junqueira, Andre B.] Wageningen Univ, Knowledge Technol & Innovat Grp, NL-6700 EW Wageningen, Netherlands.
[Junqueira, Andre B.] Inst Nacl de Pesquisas da Amazonia, Coordenacao Tecnol & Inovacao, BR-69060001 Manaus, Amazonas, Brazil.
[Kennard, Deborah] Colorado Mesa Univ, Dept Physiol & Environm Sci, Grand Junction, CO 81501 USA.
[Letcher, Susan G.] SUNY Coll Purchase, Dept Environm Studies, Purchase, NY 10577 USA.
[Licona, Juan-Carlos; Toledo, Marisol] FCA UAGRM, IBIF, Santa Cruz, Bolivia.
[Lohbeck, Madelon] World Agroforestry Ctr ICRAF, Nairobi 00100, Kenya.
[Marin-Spiotta, Erika] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA.
[Meave, Jorge A.; Mora, Francisco; Munoz, Rodrigo; Perez-Garcia, Eduardo A. .; Romero-Perez, I. Eunice] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Ecol & Recursos Nat, Mexico City 04510, DF, Mexico.
[Muscarella, Robert; Schwartz, Naomi B.; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Muscarella, Robert] Aarhus Univ, Dept Biosci, Sect Ecoinformat & Biodivers, DK-8000 Aarhus, Denmark.
[de Oliveira, Alexandre A. .] Univ Sao Paulo, Inst Biociencias, Dept Ecol, BR-05508090 Sao Paulo, Brazil.
[Piotto, Daniel] Univ Fed Sul Bahia, Ctr Formacao Ciencias Agroflorestais, BR-45613204 Itabuna, BA, Brazil.
[Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
[Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA.
[Ruiz, Jorge] UPTC, Sch Social Sci, Geog Area, Tunja, Colombia.
[Ruiz, Jorge] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Saldarriaga, Juan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Steininger, Marc K.] Yale NUS Coll, Singapore 138610, Singapore.
[Swenson, Nathan G.] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore.
[van Breugel, Michiel] El Colegio Frontera Unidad Villahermosa, Dept Agr Sociedad & Ambiente, Centro 86280, Tabasco, Mexico.
[van Breugel, Michiel] Univ Amsterdam, IBED, NL-1090 GE Amsterdam, Netherlands.
[van der Wal, Hans] Bonhoeffer Coll, NL-7545 AX Enschede, Netherlands.
[Vester, Hans F. M.] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil.
[Vester, Hans F. M.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Vieira, Ima C. G.] Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada.
RP Poorter, L (reprint author), Wageningen Univ, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
EM lourens.poorter@wur.nl
RI Dent, Daisy/L-3549-2016; Becknell, Justin/D-4577-2016; do Espirito
Santo, Mario/O-4813-2014; van der Wal, Hans/B-5621-2015; Almeida-Cortez,
Jarcilene/G-2935-2012; Craven, Dylan/K-2717-2012; Cesar,
Ricardo/I-3168-2014; Junqueira, Andre/M-1142-2016; Brancalion,
Pedro/D-6995-2012;
OI Dent, Daisy/0000-0002-1219-7344; Oliveira,
Alexandre/0000-0001-5526-8109; Meave, Jorge A./0000-0002-6241-8803; Mora
Ardila, Francisco/0000-0003-0390-0189; do Espirito Santo,
Mario/0000-0001-8274-3075; van der Wal, Hans/0000-0002-2765-8596;
Almeida-Cortez, Jarcilene/0000-0002-7118-7090; Craven,
Dylan/0000-0003-3940-833X; Junqueira, Andre/0000-0003-3681-1705;
Brancalion, Pedro/0000-0001-8245-4062; Marin-Spiotta,
Erika/0000-0001-7343-9354; Almeyda Zambrano,
Angelica/0000-0001-5081-9936
FU Australian Department of Foreign Affairs and Trade-DFAT; CGIAR-FTA;
CIFOR; Colciencias grant [243-13-16640]; Consejo Nacional de Ciencia y
Tecnologia [SEP-CONACYT 2009-129740, CONACYT 33851-B]; Conselho Nacional
de Desenvolvimento Cientifico e Tecnologico (CNPq) [563304/2010-3,
562955/2010-0, 574008/2008-0, PQ 307422/2012-7]; FOMIX-Yucatan
[YUC-2008-C06-108863]; ForestGEO; Fundacao de Amparo a Pesquisa de Minas
Gerais (FAPEMIG CRA) [APQ-00001-11]; Fundacion Ecologica de Cuixmala,
Heising-Simons Foundation; HSBC; ICETEX; Instituto Internacional de
Educacao do Brasil-IEB; Instituto Nacional de Servicos Ambientais da
Amazonia-Servamb-INPA; Inter-American Institute for Global Change
(Tropi-Dr Network) via a grant from the US National Science Foundation
[CRN3-025, GEO-1128040]; Motta Family Foundation; NASA; National Science
Foundation (NSF-CNH-RCN) [1313788]; NSF [DEB-0129104, BCS-1349952,
DEB-1053237, DEB 1050957, 0639393, 1147429, 0639114, 1147434]; NUFFIC;
USAID (BOLFOR); Science without Borders Program (CAPES/CNPq)
[88881.064976/2014-01]; Sao Paulo Research Foundation (FAPESP)
[2011/06782-5, 2014/14503-7]; Silicon Valley Foundation; Stichting Het
Kronendak; Tropenbos Foundation; University of Connecticut Research
Foundation; Wageningen University; European Union [283093]
FX This paper is a product of the 2ndFOR collaborative research network on
secondary forests. We thank the owners of the secondary forest sites for
access to their forests, all the people who have established and
measured the plots, and the institutions and funding agencies that
supported them. We thank J. Zimmerman for the use of plot data, and the
following agencies for financial support: Australian Department of
Foreign Affairs and Trade-DFAT, CGIAR-FTA, CIFOR, Colciencias grant
1243-13-16640, Consejo Nacional de Ciencia y Tecnologia (SEP-CONACYT
2009-129740 for ReSerBos, CONACYT 33851-B), Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico (CNPq: 563304/2010-3,
562955/2010-0, 574008/2008-0 and PQ 307422/2012-7), FOMIX-Yucatan
(YUC-2008-C06-108863), ForestGEO, Fundacao de Amparo a Pesquisa de Minas
Gerais (FAPEMIG CRA APQ-00001-11), Fundacion Ecologica de Cuixmala,
Heising-Simons Foundation, HSBC, ICETEX, Instituto Internacional de
Educacao do Brasil-IEB, Instituto Nacional de Servicos Ambientais da
Amazonia-Servamb-INPA, Inter-American Institute for Global Change
(Tropi-Dr Network CRN3-025) via a grant from the US National Science
Foundation (grant GEO-1128040), Motta Family Foundation, NASA
Terrestrial Ecology Program, National Science Foundation (NSF-CNH-RCN
grant 1313788 for Tropical Reforestation Network: Building a
Socioecological Understanding of Tropical Reforestation (PARTNERS), NSF
DEB-0129104, NSF BCS-1349952, NSF Career Grant DEB-1053237, NSF DEB
1050957, 0639393, 1147429, 0639114, and 1147434), NUFFIC, USAID
(BOLFOR), Science without Borders Program (CAPES/CNPq) grant number
88881.064976/2014-01, The Sao Paulo Research Foundation (FAPESP) grant
2011/06782-5 and 2014/14503-7, Silicon Valley Foundation, Stichting Het
Kronendak, Tropenbos Foundation, University of Connecticut Research
Foundation, Wageningen University (INREF Terra Preta programme and
FOREFRONT programme). This is publication number 683 in the Technical
Series of the Biological Dynamics of Forest Fragments Project
BDFFP-INPA-SI. This study was partly funded by the European Union's
Seventh Framework Programme (FP7/2007-2013) under grant agreement number
283093; Role Of Biodiversity In climate change mitigatioN (ROBIN).
NR 69
TC 45
Z9 45
U1 71
U2 181
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD FEB 11
PY 2016
VL 530
IS 7589
BP 211
EP +
DI 10.1038/nature16512
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DD4TX
UT WOS:000369916700037
PM 26840632
ER
PT J
AU Pabst, S
Lein, M
Worner, HJ
AF Pabst, Stefan
Lein, Manfred
Woerner, Hans Jakob
TI Preparing attosecond coherences by strong-field ionization
SO PHYSICAL REVIEW A
LA English
DT Article
ID MULTIPHOTON IONIZATION; CHARGE MIGRATION; LASER CONTROL; DYNAMICS;
ATOMS; IONS
AB Strong-field ionization (SFI) has been shown to prepare wave packets with few-femtosecond periods. Here, we explore whether this technique can be extended to the attosecond time scale. We introduce an intuitive model, which is based on the Fourier transform of the subcycle SFI rate, for predicting the bandwidth of ionic states that can be coherently prepared by SFI. The coherent bandwidth decreases considerably with increasing central wavelength of the ionizing pulse but it is much less sensitive to its intensity. Many-body calculations based on time-dependent configuration-interaction singles support these results. The influence of channel interactions and laser-induced dynamics within the ion is discussed. Our results further predict that multicycle femtosecond pulses can coherently prepare subfemtosecond wave packets with higher selectivity and versatility compared to single-cycle pulses with an additional sensitivity to the mutual parity of the prepared states.
C1 [Pabst, Stefan] DESY, Ctr Free Electron Laser Sci, D-22607 Hamburg, Germany.
[Pabst, Stefan] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Lein, Manfred] Leibniz Univ Hannover, Inst Theoret Phys, D-30167 Hannover, Germany.
[Lein, Manfred] Leibniz Univ Hannover, Ctr Quantum Engn & Space Time Res QUEST, D-30167 Hannover, Germany.
[Woerner, Hans Jakob] ETH, Lab Phys Chem, CH-8093 Zurich, Switzerland.
RP Pabst, S (reprint author), DESY, Ctr Free Electron Laser Sci, Notkestr 85, D-22607 Hamburg, Germany.
RI Lein, Manfred/F-4276-2011; Worner, Hans Jakob/B-1802-2013; Pabst,
Stefan/J-6541-2013
OI Lein, Manfred/0000-0003-1489-8715; Pabst, Stefan/0000-0003-1134-4629
FU Alexander von Humboldt Foundation; NSF; Helmholtz association; Deutsche
Forschungsgemeinschaft; European Research Council through an ERC
starting grant [307270-ATTOSCOPE]
FX S.P. is funded by the Alexander von Humboldt Foundation. This work was
supported by the NSF through a grant to ITAMP. S.P. thanks the Helmholtz
association for financial support through the Helmholtz Ph.D. prize.
M.L. acknowledges funding from the Deutsche Forschungsgemeinschaft.
H.J.W. gratefully acknowledges funding from the European Research
Council through an ERC starting grant (Contract No. 307270-ATTOSCOPE).
NR 39
TC 1
Z9 1
U1 7
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD FEB 11
PY 2016
VL 93
IS 2
AR 023412
DI 10.1103/PhysRevA.93.023412
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DD6FD
UT WOS:000370019100005
ER
PT J
AU Manti, S
Gallerani, S
Ferrara, A
Feruglio, C
Graziani, L
Bernardi, G
AF Manti, S.
Gallerani, S.
Ferrara, A.
Feruglio, C.
Graziani, L.
Bernardi, G.
TI Radio recombination lines from obscured quasars with the SKA
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE H II regions; Galaxy: formation; quasars: emission lines
ID SUPERMASSIVE BLACK-HOLES; YOUNG STAR-CLUSTERS; SURVEY COMMISSIONING
DATA; FALL EQUATORIAL STRIPE; HIGH-REDSHIFT GALAXIES; LUMINOSITY
FUNCTION; RUNAWAY COLLISIONS; STARBURST GALAXIES; Z-GREATER-THAN-5.7
QUASARS; Z-SIMILAR-TO-6 QUASARS
AB We explore the possibility of detecting hydrogen radio recombination lines from 0 < z < 10 quasars. We compute the expected Hn alpha flux densities as a function of absolute magnitude and redshift by considering (i) the range of observed active galactic nucleus spectral indices from UV to X-ray bands, (ii) secondary ionizations from X-ray photons, and (iii) stimulated emission due to non-thermal radiation. All these effects are important to determine the line fluxes. We find that the combination of slopes: alpha(X, hard) = -1.11, alpha(X, soft) = -0.7, alpha(EUV) = -1.3, alpha(UV) = -1.7, maximizes the expected flux, f(Hn alpha) approximate to 10 mu Jy for z similar to 7 quasars with M-AB = -27 in the n similar to 50 lines; allowed spectral energy distribution variations produce variations by a factor of 3 around this value. Secondaries boost the line intensity by a factor of 2-4, while stimulated emission in high-z quasars with M-AB approximate to -26 provides an extra boost to radio recombination line flux observed at. similar to 1 GHz if recombinations arise in H II regions with T-e approximate to 10(3-5) K, n(e) approximate to 10(3-5) cm(-3). We compute the sensitivity required for a 5 sigma detection of Hna lines using the Square Kilometre Array (SKA), finding that the SKA-MID could detect sources with M-AB less than or similar to -27 (M-AB less than or similar to -26) at z less than or similar to 8 (z less than or similar to 3) in less than 100 h of observing time. These observations could open new paths to searches for obscured SMBH progenitors, complementing X-ray, optical/IR and sub-mm surveys.
C1 [Manti, S.; Gallerani, S.; Ferrara, A.; Feruglio, C.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Graziani, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa.
[Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Manti, S (reprint author), Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
EM sere.manti@gmail.com
FU National Aeronautics and Space Administration; National Research
Foundation [92725]; European Research Council under the European Union
[306476]
FX This research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration.; This work is based on research supported by the
National Research Foundation under grant 92725. Any opinion, finding and
conclusion or recommendation expressed in this material is that of the
author(s) and the NRF does not accept any liability in this regard.; LG
acknowledges the support of the European Research Council under the
European Union (FP/2007-2013)/ERC Grant Agreement n. 306476.
NR 103
TC 0
Z9 0
U1 1
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP 98
EP 107
DI 10.1093/mnras/stv2635
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000037
ER
PT J
AU Xu, DD
Sluse, D
Schneider, P
Springel, V
Vogelsberger, M
Nelson, D
Hernquist, L
AF Xu, Dandan
Sluse, Dominique
Schneider, Peter
Springel, Volker
Vogelsberger, Mark
Nelson, Dylan
Hernquist, Lars
TI Lens galaxies in the Illustris simulation: power-law models and the bias
of the Hubble constant from time delays
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: haloes; galaxies: structure;
cosmology: theory; dark matter
ID MASS DENSITY PROFILE; TO-LIGHT RATIOS; GRAVITATIONAL LENS; DARK-MATTER;
SLACS LENSES; ACS SURVEY; 2-DIMENSIONAL KINEMATICS; SUPERNOVAE;
EVOLUTION; DYNAMICS
AB A power-law density model, i.e. rho(r) proportional to r(-gamma)', has been commonly employed in strong gravitational lensing studies, including the so-called time-delay technique used to infer the Hubble constant H-0. However, since the radial scale at which strong lensing features are formed corresponds to the transition from the dominance of baryonic matter to dark matter, there is no known reason why galaxies should follow a power law in density. The assumption of a power law artificially breaks the mass-sheet degeneracy, a well-known invariance transformation in gravitational lensing which affects the product of Hubble constant and time delay and can therefore cause a bias in the determination of H-0 from the time-delay technique. In this paper, we use the Illustris hydrodynamical simulations to estimate the amplitude of this bias, and to understand how it is related to observational properties of galaxies. Investigating a large sample of Illustris galaxies that have velocity dispersion sigma(SIE) >= 160 km s(-1) at redshifts below z = 1, we find that the bias on H-0 introduced by the power-law assumption can reach 20-50 per cent, with a scatter of 10-30 per cent (rms). However, we find that by selecting galaxies with an inferred power-law model slope close to isothermal, it is possible to reduce the bias on H-0 to less than or similar to 5 per cent and the scatter to less than or similar to 10 per cent. This could potentially be used to form less biased statistical samples for H-0 measurements in the upcoming large survey era.
C1 [Xu, Dandan; Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
[Sluse, Dominique] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Schneider, Peter] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Vogelsberger, Mark] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nelson, Dylan] Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Xu, DD (reprint author), Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany.
EM Dandan.Xu@h-its.org
FU HITS fellowship; Belgian Federal Science Policy (BELSPO); Deutsche
Forschungsgemeinschaft [SL172/1-1]; DFG [Transregio 33]; European
Research Council [ERC-StG EXAGAL-308037]; NASA [NNX12AC67G]; NSF
[AST-1312095]; Klaus Tschira Foundation
FX The authors would like to thank Stefan Hilbert, Sherry Suyu, Malte
Tewes, James Nightingale and an anonymous referee for very useful
comments. DDX thanks the HITS fellowship. DS acknowledges support from a
Back to Belgium grant from the Belgian Federal Science Policy (BELSPO)
and partial funding from the Deutsche Forschungsgemeinschaft, reference
SL172/1-1. PS and VS acknowledge support by the DFG through Transregio
33, 'The Dark Universe'. VS also acknowledges support by the European
Research Council under ERC-StG EXAGAL-308037. LH acknowledges support
from NASA grant NNX12AC67G and NSF grant AST-1312095. DDX and VS
gratefully acknowledge the support of the Klaus Tschira Foundation.
NR 47
TC 9
Z9 9
U1 1
U2 6
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP 739
EP 755
DI 10.1093/mnras/stv2708
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000091
ER
PT J
AU Bruderer, C
Read, JI
Coles, JP
Leier, D
Falco, EE
Ferreras, I
Saha, P
AF Bruderer, Claudio
Read, Justin I.
Coles, Jonathan P.
Leier, Dominik
Falco, Emilio E.
Ferreras, Ignacio
Saha, Prasenjit
TI Light versus dark in strong-lens galaxies: dark matter haloes that are
rounder than their stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: elliptical and lenticular, cD;
galaxies: formation; galaxies: haloes; galaxies: structure
ID INITIAL MASS FUNCTION; 4-IMAGE GRAVITATIONAL LENS; FLUX RATIO; CHANDRA
OBSERVATIONS; INTERNAL STRUCTURE; FUNDAMENTAL PLANE; GROUP CONNECTION;
RX J0911.4+0551; TIDAL STREAMS; MG 0414+0534
AB We measure the projected density profile, shape and alignment of the stellar and dark matter mass distribution in 11 strong-lens galaxies. We find that the projected dark matter density profile - under the assumption of a Chabrier stellar initial mass function - shows significant variation from galaxy to galaxy. Those with an outermost image beyond similar to 10 kpc are very well fit by a projected Navarro-Frenk-White (NFW) profile; those with images within 10 kpc appear to be more concentrated than NFW, as expected if their dark haloes contract due to baryonic cooling. We find that over several half-light radii, the dark matter haloes of these lenses are rounder than their stellar mass distributions. While the haloes are never more elliptical than e(dm) = 0.2, their stars can extend to e(*) > 0.2. Galaxies with high dark matter ellipticity and weak external shear show strong alignment between light and dark; those with strong shear (gamma greater than or similar to 0.1) can be highly misaligned. This is reassuring since isolated misaligned galaxies are expected to be unstable. Our results provide a new constraint on galaxy formation models. For a given cosmology, these must explain the origin of both very round dark matter haloes and misaligned strong-lens systems.
C1 [Bruderer, Claudio; Read, Justin I.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Read, Justin I.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England.
[Coles, Jonathan P.] Exascale Res Comp Lab, F-91680 Bruyeres Le Chatel, France.
[Coles, Jonathan P.; Saha, Prasenjit] Univ Zurich, Inst Phys, CH-8057 Zurich, Switzerland.
[Leier, Dominik] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ferreras, Ignacio] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Saha, Prasenjit] Univ Zurich, Inst Computat Sci, CH-8057 Zurich, Switzerland.
RP Bruderer, C (reprint author), ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
EM claudio.bruderer@phys.ethz.ch
OI Ferreras, Ignacio/0000-0003-4584-3127
FU SNF [PP00P2_128540/1]; European Seventh Framework Programme, Ideas
[259349]
FX We thank Simon Birrer and William Hartley for useful discussion. JIR
would like to acknowledge support from SNF grant PP00P2_128540/1. DL's
research is part of the project GLENCO, funded under the European
Seventh Framework Programme, Ideas, Grant Agreement no. 259349.
NR 113
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP 870
EP 884
DI 10.1093/mnras/stv2582
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000100
ER
PT J
AU Blecha, L
Sijacki, D
Kelley, LZ
Torrey, P
Vogelsberger, M
Nelson, D
Springel, V
Snyder, G
Hernquist, L
AF Blecha, Laura
Sijacki, Debora
Kelley, Luke Zoltan
Torrey, Paul
Vogelsberger, Mark
Nelson, Dylan
Springel, Volker
Snyder, Gregory
Hernquist, Lars
TI Recoiling black holes: prospects for detection and implications of spin
alignment
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ccretion, accretion discs; black hole physics; gravitational waves;
hydrodynamics; galaxies: active; galaxies: interactions
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; GRAVITATIONAL-WAVE RECOIL;
QUASAR SDSS J092712.65+294344.0; GALAXY FORMATION PHYSICS; PULSAR TIMING
ARRAYS; COSMOLOGICAL SIMULATIONS; ACCRETION DISKS; MERGER REMNANTS;
HYDRODYNAMICAL SIMULATIONS
AB Supermassive black hole (BH) mergers produce powerful gravitational wave emission. Asymmetry in this emission imparts a recoil kick to the merged BH, which can eject the BH from its host galaxy altogether. Recoiling BHs could be observed as offset active galactic nuclei (AGN). Several candidates have been identified, but systematic searches have been hampered by large uncertainties regarding their observability. By extracting merging BHs and host galaxy properties from the Illustris cosmological simulations, we have developed a comprehensive model for recoiling AGN. Here, for the first time, we model the effects of BH spin alignment and recoil dynamics based on the gas richness of host galaxies. We predict that if BH spins are not highly aligned, seeing-limited observations could resolve offset AGN, making them promising targets for all-sky surveys. For randomly oriented spins, less than or similar to 10 spatially offset AGN may be detectable in Hubble Space Telescope-Cosmological Evolution Survey, and >10(3) could be found with the Panoramic Survey Telescope & Rapid Response System (Pan-STARRS), the Large Synoptic Survey Telescope (LSST), Euclid, and the Wide-Field Infrared Survey Telescope (WFIRST). Nearly a thousand velocity offset AGN are predicted within the Sloan Digital Sky Survey (SDSS) footprint; the rarity of large broad-line offsets among SDSS quasars is likely due in part to selection effects but suggests that spin alignment plays a role in suppressing recoils. None the less, in our most physically motivated model where alignment occurs only in gas-rich mergers, hundreds of offset AGN should be found in all-sky surveys. Our findings strongly motivate a dedicated search for recoiling AGN.
C1 [Blecha, Laura] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Kelley, Luke Zoltan; Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Torrey, Paul; Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA.
[Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
[Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany.
[Snyder, Gregory] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Blecha, L (reprint author), Univ Maryland, Dept Astron, 1113 PSC,Bldg 415, College Pk, MD 20742 USA.
EM lblecha@astro.umd.edu
FU NASA [PF2-130093, NNX12AC67G]; NSF [AST-1312095]; European Research
Council through ERC-StG grant [EXAGAL-308037]; PRACE project [RA0844];
Leibniz Computing Centre, Germany [pr85je]
FX We would like to thank Cole Miller, Suvi Gezari, and Julie Comerford for
useful discussions and comments on the manuscript, and we also thank
Enrico Barausse, Marta Volonteri, and Alberto Sesana for helpful
discussions and comparisons with their model data. LB acknowledges
support provided by NASA through Einstein Fellowship grant PF2-130093.
LH acknowledges support from NASA grant NNX12AC67G and NSF grant
AST-1312095. VS acknowledges support through the European Research
Council through ERC-StG grant EXAGAL-308037. Simulations were run on the
Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede
supercomputers at the Texas Advanced Computing Center as part of XSEDE,
the Kraken supercomputer at Oak Ridge National Laboratory as part of
XSEDE, the CURIE supercomputer at CEA/France as part of PRACE project
RA0844, and the SuperMUC computer at the Leibniz Computing Centre,
Germany, as part of project pr85je.
NR 141
TC 8
Z9 8
U1 2
U2 13
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP 961
EP 989
DI 10.1093/mnras/stv2646
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000106
ER
PT J
AU Wellons, S
Torrey, P
Ma, CP
Rodriguez-Gomez, V
Pillepich, A
Nelson, D
Genel, S
Vogelsberger, M
Hernquist, L
AF Wellons, Sarah
Torrey, Paul
Ma, Chung-Pei
Rodriguez-Gomez, Vicente
Pillepich, Annalisa
Nelson, Dylan
Genel, Shy
Vogelsberger, Mark
Hernquist, Lars
TI The diverse evolutionary paths of simulated high-z massive, compact
galaxies to z=0
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift
ID SIMILAR-TO 2; HIGH-REDSHIFT GALAXIES; QUIESCENT GALAXIES; COSMOLOGICAL
SIMULATIONS; ILLUSTRIS SIMULATION; ELLIPTIC GALAXIES; SIZE EVOLUTION;
BLACK-HOLES; VELOCITY-DISPERSION; STAR-FORMATION
AB Massive quiescent galaxies have much smaller physical sizes at high redshift than today. The strong evolution of galaxy size may be caused by progenitor bias, major and minor mergers, adiabatic expansion, and/or renewed star formation, but it is difficult to test these theories observationally. Herein, we select a sample of 35 massive, compact galaxies (M* = 1-3 x 10(11) M-circle dot, M*/R-1.5 > 10(10.5) M-circle dot/kpc(1.5)) at z = 2 in the cosmological hydrodynamical simulation Illustris and trace them forwards to z = 0 to uncover their evolution and identify their descendants. By z= 0, the original factor of 3 difference in stellarmass spreads to a factor of 20. The dark matter halo masses similarly spread from a factor of 5 to 40. The galaxies' evolutionary paths are diverse: about half acquire an ex situ envelope and are the core of a more massive descendant, a third survive undisturbed and gain very little mass, 15 per cent are consumed in a merger with a more massive galaxy, and a small remainder are thoroughly mixed by major mergers. The galaxies grow in size as well as mass, and only similar to 10 per cent remain compact by z = 0. The majority of the size growth is driven by the acquisition of ex situ mass. The most massive galaxies at z = 0 are the most likely to have compact progenitors, but this trend possesses significant dispersion which precludes a direct linkage to compact galaxies at z = 2. The compact galaxies' merger rates are influenced by their z = 2 environments, so that isolated or satellite compact galaxies (which are protected from mergers) are the most likely to survive to the present day.
C1 [Wellons, Sarah; Rodriguez-Gomez, Vicente; Pillepich, Annalisa; Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Torrey, Paul; Vogelsberger, Mark] MIT, Cambridge, MA 02139 USA.
[Torrey, Paul] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Ma, Chung-Pei] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Genel, Shy] Columbia Univ, Dept Astron, New York, NY 10027 USA.
RP Wellons, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM swellons@cfa.harvard.edu
OI Rodriguez-Gomez, Vicente/0000-0002-9495-0079
FU National Science Foundation [DGE1144152]; NASA ATP [NNX14AH35G]; NASA
[NNX11AI97G, NAS5-26555, NNX12AC67G]; NSF [AST-1411945, AST-1312095];
HST [HST-AR-13897]; NASA - STScI [HST-HF2-51341.001-A]
FX SW is supported by the National Science Foundation Graduate Research
Fellowship under grant number DGE1144152. PT acknowledges support from
NASA ATP Grant NNX14AH35G. CPM acknowledges support from NASA grant
NNX11AI97G and NSF grant AST-1411945. AP acknowledges support from the
HST grant HST-AR-13897. SG acknowledges support provided by NASA through
Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which
is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS5-26555. LH acknowledges
support from NASA grant NNX12AC67G and NSF grant AST-1312095.
NR 75
TC 12
Z9 12
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP 1030
EP 1048
DI 10.1093/mnras/stv2738
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000110
ER
PT J
AU Marinucci, A
Bianchi, S
Matt, G
Alexander, DM
Balokovic, M
Bauer, FE
Brandt, WN
Gandhi, P
Guainazzi, M
Harrison, FA
Iwasawa, K
Koss, M
Madsen, KK
Nicastro, F
Puccetti, S
Ricci, C
Stern, D
Walton, DJ
AF Marinucci, A.
Bianchi, S.
Matt, G.
Alexander, D. M.
Balokovic, M.
Bauer, F. E.
Brandt, W. N.
Gandhi, P.
Guainazzi, M.
Harrison, F. A.
Iwasawa, K.
Koss, M.
Madsen, K. K.
Nicastro, F.
Puccetti, S.
Ricci, C.
Stern, D.
Walton, D. J.
TI NuSTAR catches the unveiling nucleus of NGC 1068
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: NGC 1068; galaxies: Seyfert
ID X-RAY SOURCE; ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; XMM-NEWTON;
LINE COMPLEX; BROAD-BAND; NGC-1068; EMISSION; REFLECTION; ABSORBERS
AB We present a NuSTAR and XMM-Newton monitoring campaign in 2014/2015 of the Compton-thick Seyfert 2 galaxy, NGC 1068. During the 2014 August observation, we detect with NuSTAR a flux excess above 20 keV (32 +/- 6 per cent) with respect to the 2012 December observation and to a later observation performed in 2015 February. We do not detect any spectral variation below 10 keV in the XMM-Newton data. The transient excess can be explained by a temporary decrease of the column density of the obscuring material along the line of sight (from N-H similar or equal to 10(25) cm(-2) to N-H = 6.7 +/- 1.0 x 10(24) cm(-2)), which allows us for the first time to unveil the direct nuclear radiation of the buried active galactic nucleus in NGC 1068 and to infer an intrinsic 2-10 keV luminosity L-X = 7(-4)(+7) x 10(43) erg s(-1).
C1 [Marinucci, A.; Bianchi, S.; Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Alexander, D. M.; Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Balokovic, M.; Harrison, F. A.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Guainazzi, M.] European Space Astron Ctr ESA, E-28691 Madrid, Spain.
[Iwasawa, K.] Univ Barcelona, IEEC UB, ICREA, E-08028 Barcelona, Spain.
[Iwasawa, K.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Nicastro, F.; Puccetti, S.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
[Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nicastro, F.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece.
[Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Marinucci, A (reprint author), Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
EM marinucci@fis.uniroma3.it
RI Bianchi, Stefano/B-4804-2010
OI Bianchi, Stefano/0000-0002-4622-4240
FU Italian Space Agency [ASI/INAF I/037/12/0-011/13]; CONICYT-Chile
[PFB-06/2007, FONDECYT 1141218, ACT1101, IC120009]; Caltech NuSTAR
[44A-1092750]; STFC [ST/J003697/1]; NASA [NNG08FD60C, NNX10AC99G,
NNX14AQ07H]; National Aeronautics and Space Administration
FX We thank the referee for her/his comments. AM, SB and GM acknowledge
financial support from Italian Space Agency under grant ASI/INAF
I/037/12/0-011/13. FEB acknowledges support from CONICYT-Chile
(PFB-06/2007, FONDECYT 1141218, ACT1101), and grant IC120009, awarded to
The Millennium Institute of Astrophysics, MAS. WNB acknowledges Caltech
NuSTAR subcontract 44A-1092750. PG thanks STFC for support (grant
reference ST/J003697/1). This work was supported under NASA Contracts
No. NNG08FD60C, NNX10AC99G, NNX14AQ07H and made use of data from the
NuSTAR mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the National
Aeronautics and Space Administration. We thank the NuSTAR Operations,
Software and Calibration teams for support with the execution and
analysis of these observations. This research has made use of the NuSTAR
Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(USA).
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 11
PY 2016
VL 456
IS 1
BP L94
EP L98
DI 10.1093/mnrasl/slv178
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UN
UT WOS:000368010000020
ER
PT J
AU Arevalo, P
Churazov, E
Zhuravleva, I
Forman, WR
Jones, C
AF Arevalo, P.
Churazov, E.
Zhuravleva, I.
Forman, W. R.
Jones, C.
TI ON THE NATURE OF X-RAY SURFACE BRIGHTNESS FLUCTUATIONS IN M87
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (M87/Virgo); galaxies: clusters:
intracluster medium; X-rays: galaxies: clusters
ID ANISOTROPIC THERMAL CONDUCTION; GAS-DENSITY FLUCTUATIONS; JET-INFLATED
BUBBLES; INTRACLUSTER MEDIUM; PERSEUS CLUSTER; GALAXY CLUSTERS; VIRGO
CLUSTER; HIGH-RESOLUTION; GASEOUS ATMOSPHERE; COOLING FLOWS
AB X-ray images of galaxy clusters and gas-rich elliptical galaxies show a wealth of small-scale features that reflect fluctuations in density and/or temperature of the intracluster medium. In this paper we study these fluctuations in M87/Virgo to establish whether sound waves/shocks, bubbles, or uplifted cold gas dominate the structure. We exploit the strong dependence of the emissivity on density and temperature in different energy bands to distinguish between these processes. Using simulations we demonstrate that our analysis recovers the leading type of fluctuation even in the presence of projection effects and temperature gradients. We confirm the isobaric nature of cool filaments of gas entrained by buoyantly rising bubbles, extending to 7' to the east and southwest, and the adiabatic nature of the weak shocks at 40 '' and 3' from the center. For features of similar to 5-10 kpc, we show that the central 4' x 4' region is dominated by cool structures in pressure equilibrium with the ambient hotter gas while up to 30% of the variance in this region can be ascribed to adiabatic fluctuations. The remaining part of the central 14' x 14' region, excluding the arms and shocks described above, is dominated by apparently isothermal fluctuations (bubbles) with a possible admixture (at the level of similar to 30%) of adiabatic (sound waves) and by isobaric structures. Larger features, of about 30 kpc, show a stronger contribution from isobaric fluctuations. The results broadly agree with a model based on feedback from an active galactic nucleus mediated by bubbles of relativistic plasma.
C1 [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
[Churazov, E.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Churazov, E.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Zhuravleva, I.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.
[Zhuravleva, I.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Forman, W. R.; Jones, C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Arevalo, P (reprint author), Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
RI Churazov, Eugene/A-7783-2013
FU Fondecyt grant [1140304]; Centro de Astrofisica de Valparaiso (CAV);
Smithsonian Astrophysical Observatory; NASA-Chandra [AR1-12007X]
FX We are grateful to Alex Schekochihin for numerous discussions and the
anonymous referee for useful suggestions that helped to improve the
paper. P.A. acknowledges support from Fondecyt grant 1140304 and the
Centro de Astrofisica de Valparaiso (CAV). W.F. acknowledges support
from the Smithsonian Astrophysical Observatory and NASA-Chandra archive
proposal AR1-12007X.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 14
DI 10.3847/0004-637X/818/1/14
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800014
ER
PT J
AU Fesen, RA
Milisavljevic, D
AF Fesen, Robert A.
Milisavljevic, Dan
TI AN HST SURVEY OF THE HIGHEST-VELOCITY EJECTA IN CASSIOPEIA A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Cassiopeia A); ISM: kinematics and dynamics
ID SUPERNOVA REMNANT CASSIOPEIA; CORE-COLLAPSE SUPERNOVA; GAMMA-RAY BURST;
X-RAY; PROPER MOTIONS; A SUPERNOVA; SN 2012AP; RELATIVISTIC SUPERNOVAE;
3-DIMENSIONAL STRUCTURE; STELLAR-EXPLOSIONS
AB We present Hubble Space Telescope WFC3/IR images of the Cassiopeia A supernova remnant that survey its high-velocity, S-rich debris in the NE jet and SW counterjet regions through [S III] lambda lambda 9069, 9531 and [S II] lambda lambda 10,287-10,370 line emissions. We identify nearly 3400 sulfur emitting knots concentrated in similar to 120 degrees wide opposing streams, almost triple the number previously known. The vast majority of these ejecta knots lie at projected distances well out ahead of the remnant's forward blast wave and main shell ejecta, extending to angular distance of 320 '' to the NE and 260 '' to the SW from the center of expansion. Such angular distances imply undecelerated ejecta knot transverse velocities of 15,600 and 12,700 km s(-1), respectively, assuming an explosion date approximate to 1670 AD and a distance of 3.4 kpc. Optical spectra of knots near the outermost tip of the NE ejecta stream show strong emission lines of S, Ca, and Ar. We estimate a total mass similar to 0.1 M-circle dot and a kinetic energy of at least similar to 1 x 10(50) erg for S-rich ejecta in the NE jet and SW counterjet. Although their broadness and kinetic energy argue against the Cas. A SN being a jet-induced explosion, the jets are kinematically and chemically distinct from the rest of the remnant. This may reflect an origin in a jet-like mechanism that accelerated interior material from a Si-, S-, Ar-, and Ca-rich region near the progenitor's core up through the mantle and H-, He-, N-, and O-rich outer layers with velocities that greatly exceeded that of the rapidly expanding photosphere.
C1 [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA.
[Milisavljevic, Dan] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Fesen, RA (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA.
FU NASA from the Space Telescope Science Institute (STScI) [GO-12300,
GO-12674]
FX We thank D. Patnaude for helpful discussions about Cas A, the staffs of
MDM and MMT Observatories for observing support that made the
ground-based observations possible, C. Black for assistance with the
optical spectra, and the referee for helpful comments. This work was
supported by NASA through grants GO-12300 and GO-12674 from the Space
Telescope Science Institute (STScI), which is operated by the
Association of Universities for Research in Astronomy. A portion of the
observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800017
ER
PT J
AU Flaherty, KM
Hughes, AM
Andrews, SM
Qi, CH
Wilner, DJ
Boley, AC
White, JA
Harney, W
Zachary, J
AF Flaherty, Kevin M.
Hughes, A. Meredith
Andrews, Sean M.
Qi, Chunhua
Wilner, David J.
Boley, Aaron C.
White, Jacob A.
Harney, Will
Zachary, Julia
TI RESOLVED CO GAS INTERIOR TO THE DUST RINGS OF THE HD 141569 DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: individual (HD 141569)
ID MAIN-SEQUENCE STARS; A-TYPE STARS; ICY PLANET FORMATION; HERBIG AEBE
STARS; BETA-PICTORIS; DEBRIS DISK; CIRCUMSTELLAR DISK; MOLECULAR GAS;
PROTOPLANETARY DISCS; INFRARED-EMISSION
AB The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.
C1 [Flaherty, Kevin M.; Hughes, A. Meredith; Zachary, Julia] Wesleyan Univ, Dept Astron, Van Vleck Observ, 96 Foss Hill Dr, Middletown, CT 06459 USA.
[Andrews, Sean M.; Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Boley, Aaron C.; White, Jacob A.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Harney, Will] Union Coll, Dept Phys & Astron, Schenectady, NY 12308 USA.
RP Flaherty, KM (reprint author), Wesleyan Univ, Dept Astron, Van Vleck Observ, 96 Foss Hill Dr, Middletown, CT 06459 USA.
OI White, Jacob/0000-0001-8445-0444
FU NSF [AST-1412647]; Smithsonian Institution; James S. McDonnell
Foundation; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L.
Norris Foundation; University of Chicago; Associates of the California
Institute of Technology; National Science Foundation; CARMA partner
universities; Academia Sinica; state of California; state of Illinois;
state of Maryland
FX We thank the referee for helpful comments regarding the context and
interpretation of our results. We gratefully acknowledge support from
NSF grant AST-1412647. The Submillimeter Array is a joint project
between the Smithsonian Astrophysical Observatory and the Academia
Sinica Institute of Astronomy and Astrophysics and is funded by the
Smithsonian Institution and the Academia Sinica. The authors wish to
recognize and acknowledge the very significant cultural role and
reverance that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. This research
made use of Astropy, a community-developed core Python package for
Astronomy (Astropy Collaboration et al. 2013). Support for CARMA
construction was derived from the states of California, Illinois, and
Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the
University of Chicago, the Associates of the California Institute of
Technology, and the National Science Foundation. CARMA development and
operations were supported by the National Science Foundation under a
cooperative agreement, and by the CARMA partner universities.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800097
ER
PT J
AU Hargis, JR
Kimmig, B
Willman, B
Caldwell, N
Walker, MG
Strader, J
Sand, DJ
Grillmair, CJ
Yoon, JH
AF Hargis, Jonathan R.
Kimmig, Brian
Willman, Beth
Caldwell, Nelson
Walker, Matthew G.
Strader, Jay
Sand, David J.
Grillmair, Carl J.
Yoon, Joo Heon
TI EVIDENCE THAT HYDRA I IS A TIDALLY DISRUPTING MILKY WAY DWARF GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; Galaxy: halo; Galaxy: structure
ID DIGITAL SKY SURVEY; EXPLORING HALO SUBSTRUCTURE; DARK ENERGY SURVEY;
GLOBULAR-CLUSTERS; ANTICENTER STREAM; MAGELLANIC-CLOUD; STELLAR SPECTRA;
GALACTIC HALO; METALLICITY RELATION; SPHEROIDAL GALAXIES
AB The Eastern Banded Structure (EBS) and Hydra. I halo overdensities are very nearby (d similar to 10 kpc) objects discovered in Sloan Digital Sky Survey (SDSS) data. Previous studies of the region have shown that EBS and Hydra I are spatially coincident, cold structures at the same distance, suggesting that Hydra I may be the EBS's progenitor. We combine new wide-field Dark Energy Camera (DECam) imaging and MMT/Hectochelle spectroscopic observations of Hydra I with SDSS archival spectroscopic observations to quantify Hydra I's present-day chemodynamical properties, and to infer whether it originated as a star cluster or dwarf galaxy. While previous work using shallow SDSS imaging assumed a standard old, metal-poor stellar population, our deeper DECam imaging reveals that Hydra. I has a thin, well-defined main sequence turnoff of intermediate age (similar to 5-6 Gyr) and metallicity ([Fe/H] = -0.9 dex). We measure statistically significant spreads in both the iron and alpha-element abundances of sigma([Fe/H]) = 0.13 +/- 0.02 dex and sigma([alpha/Fe]) = 0.09 +/- 0.03 dex, respectively, and place upper limits on both the rotation and its proper motion. Hydra I's intermediate age and [Fe/H]-as well as its low [alpha/Fe], apparent [Fe/H] spread, and present-day low luminosity-suggest that its progenitor was a dwarf galaxy, which has subsequently lost more than 99.99% of its stellar mass.
C1 [Hargis, Jonathan R.; Kimmig, Brian; Willman, Beth] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA.
[Willman, Beth] LSST, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Willman, Beth] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Walker, Matthew G.] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
[Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Sand, David J.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA.
[Grillmair, Carl J.] Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Yoon, Joo Heon] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Hargis, JR (reprint author), Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA.
FU NSF Faculty Early Career Development (CAREER) award [AST-1151462];
National Science Foundation [AST-1313045, AST-1412999, PHYS-1066293];
NSF [AST-1514763]; DOE; NSF (USA); MISE(Spain); STFC(UK); HEFCE(UK)
FX B.W., J.R.H., and B.K. were supported by an NSF Faculty Early Career
Development (CAREER) award (AST-1151462). M.G.W. is supported by
National Science Foundation grants AST-1313045, AST-1412999. J.S.
acknowledges support from NSF grant AST-1514763. J.R.H. would like to
acknowledge useful conversations with Keith Hawkins, Ting Li, and
Jennifer Marshall during the course of this work. J.R.H. would also like
to thank Kathy Vivas both for useful conversations and observing support
during the DECam observing at CTIO. We thank the anonymous referee for
very helpful comments on the manuscript. This work was supported in part
by National Science Foundation Grant No. PHYS-1066293 and the
hospitality of the Aspen Center for Physics. This project used data
obtained with the Dark Energy Camera, which was constructed by the Dark
Energy Survey collaboration. Funding for the DES Projects has been
provided by the DOE and NSF (USA), MISE(Spain), STFC(UK), HEFCE(UK).
NCSA (UIUC), KICP(U. Chicago), CCAPP(Ohio State), MIFPA (Texas A&M),
CNPQ, FAPERJ, FINEP (Brazil), MINECO (Spain), DFG(Germany) and the
collaborating institutions in the Dark Energy Survey, which are Argonne
Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University
of Chicago, University College London, DES-Brazil Consortium, University
of Edinburgh, ETH Zurich, Fermilab, University of Illinois, ICE
(IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU Munchen and the
associated Excellence Cluster universe, University of Michigan, NOAO,
University of Nottingham, Ohio State University, University of
Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford
University, University of Sussex, and Texas A&M University.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800039
ER
PT J
AU Kashiyama, K
Murase, K
Bartos, I
Kiuchi, K
Margutti, R
AF Kashiyama, Kazumi
Murase, Kohta
Bartos, Imre
Kiuchi, Kenta
Margutti, Raffaella
TI MULTI-MESSENGER TESTS FOR FAST-SPINNING NEWBORN PULSARS EMBEDDED IN
STRIPPED-ENVELOPE SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; stars: magnetars; supernovae: general; X-rays:
general
ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; ISOLATED RADIO PULSARS;
NEUTRON-STARS; LIGHT CURVES; IC SUPERNOVAE; WIND NEBULAE; SUPERLUMINOUS
SUPERNOVAE; GRAVITATIONAL-RADIATION; ASYMMETRIC SUPERNOVAE
AB Fast-spinning strongly magnetized newborn neutron stars (NSs), including nascent magnetars, are popularly implemented as the engine of luminous stellar explosions. Here, we consider the scenario that they power various stripped-envelope (SE) supernovae (SNe), not only superluminous SNe Ic but also broad-line (BL) SNe Ibc and possibly some ordinary SNe Ibc. This scenario is also motivated by the hypothesis that Galactic magnetars largely originate from fast-spinning NSs as remnants of SE SNe. By consistently modeling the energy injection from magnetized wind and Ni-56 decay, we show that proto-NSs with greater than or similar to 10 ms rotation and a poloidal magnetic field of B-dip greater than or similar to 5 x 10(14) G can be harbored in ordinary SNe Ibc. On the other hand, millisecond proto-NSs can solely power BL SNe Ibc if they are born with B-dip greater than or similar to 5 x 10(14) G and superluminous SNe Ic with B-dip greater than or similar to 10(13) G. Then, we study how multi-messenger emission can be used to discriminate such pulsar-driven SN models from other competitive scenarios. First, high-energy X-ray and gamma-ray emission from embryonic pulsar wind nebulae can probe the underlying newborn pulsar. Follow-up observations of SE SNe using NuSTAR similar to 50-100 days after the explosion are strongly encouraged for nearby objects. We also discuss possible effects of gravitational waves (GWs) on the spin-down of proto-NSs. If millisecond proto-NSs with B-dip < a few x 10(13) G emit GWs through, e.g., non-axisymmetric rotation deformed by the inner toroidal fields of B-t greater than or similar to 10(16) G, the GW signal can be detectable from ordinary SNe Ibc in the Virgo cluster by Advanced LIGO, Advanced Virgo, and KAGRA.
C1 [Kashiyama, Kazumi] Univ Calif Berkeley, Dept Phys, Theoret Astrophys Ctr, Dept Astron, Berkeley, CA 94720 USA.
[Murase, Kohta] Inst Adv Study, Sch Nat Sci, 1 Einstein Dr, Princeton, NJ 08540 USA.
[Murase, Kohta] Penn State Univ, Dept Astron & Astrophys, Dept Phys, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA.
[Bartos, Imre] Columbia Univ, Dept Phys, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kiuchi, Kenta] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan.
[Margutti, Raffaella] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Kashiyama, K (reprint author), Univ Calif Berkeley, Dept Phys, Theoret Astrophys Ctr, Dept Astron, Berkeley, CA 94720 USA.
RI Bartos, Imre/A-2592-2017; Murase, Kohta/B-2710-2016
OI Murase, Kohta/0000-0002-5358-5642
FU NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center
[PF4-150123]; NASA [NAS8-03060]; HPCI Strategic Program of Japanese
MEXT/JSPS [hpci130025, 140211, 150225]; Columbia University in New York
City; National Science Foundation [PHY-1404462]
FX This work is supported by NASA through Einstein Postdoctoral Fellowship
grant number PF4-150123 awarded by the Chandra X-ray Center, which is
operated by the Smithsonian Astrophysical Observatory for NASA under
contract NAS8-03060 (K. Kashiyama). K.M. acknowledges continuous support
from the Institute for Advanced Study and Pennsylvania State University.
K. Kiuchi is supported by a Grant-in-Aid for Scientific Research
(15H00783, 15H00836, 15K05077) and by HPCI Strategic Program of Japanese
MEXT/JSPS (Project numbers hpci130025, 140211, and 150225). I.B. is
thankful for the generous support of Columbia University in New York
City and the National Science Foundation under cooperative agreement
PHY-1404462.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 94
DI 10.3847/0004-637X/818/1/94
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800094
ER
PT J
AU LaMassa, SM
Civano, F
Brusa, M
Stern, D
Glikman, E
Gallagher, S
Urry, CM
Cales, S
Cappelluti, N
Cardamone, C
Comastri, A
Farrah, D
Greene, JE
Komossa, S
Merloni, A
Mroczkowski, T
Natarajan, P
Richards, G
Salvato, M
Schawinski, K
Treister, E
AF LaMassa, Stephanie M.
Civano, Francesca
Brusa, Marcella
Stern, Daniel
Glikman, Eilat
Gallagher, Sarah
Urry, C. Meg
Cales, Sabrina
Cappelluti, Nico
Cardamone, Carolin
Comastri, Andrea
Farrah, Duncan
Greene, Jenny E.
Komossa, S.
Merloni, Andrea
Mroczkowski, Tony
Natarajan, Priyamvada
Richards, Gordon
Salvato, Mara
Schawinski, Kevin
Treister, Ezequiel
TI ON R-W1 AS A DIAGNOSTIC TO DISCOVER OBSCURED ACTIVE GALACTIC NUCLEI IN
WIDE-AREA X-RAY SURVEYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; infrared: galaxies; quasars: general; quasars:
supermassive black holes; X-rays: galaxies; X-rays: general
ID DIGITAL SKY SURVEY; DEEP FIELD-SOUTH; XMM-NEWTON OBSERVATIONS;
SIMILAR-TO 2; OSCILLATION SPECTROSCOPIC SURVEY; OPTICALLY NORMAL
GALAXIES; EMISSION-LINE GALAXIES; DUST-REDDENED QUASARS; CHANDRA-COSMOS
SURVEY; 10TH DATA RELEASE
AB Capitalizing on the all-sky coverage of WISE. and the 35% and 50% sky coverage from Sloan Digital Sky Survey and Pan-STARRS, respectively, we explore the efficacy of m(R) (optical) - m(3.4 mu m) (mid-infrared), hereafter R - W1, as a color diagnostic to identify obscured supermassive black hole accretion in wide-area X-ray surveys. We use the similar to 16.5 deg(2) Stripe 82 X-ray survey data as a test. bed to compare R - W1 with R - K, an oft-used obscured active galactic nucleus (AGN) selection criterion, and examine where different classes of objects lie in this parameter space. Most stars follow a well-defined path in R - K versus R - W1 space. We demonstrate that optically normal galaxies hosting X-ray AGNs at redshifts 0.5 < z < 1 can be recovered with an R - W1 > 4 color cut, while they typically are not selected as AGNs based on their W1 - W2 colors. Additionally, different observed X-ray luminosity bins favor different regions in R - W1 parameter space: moderate-luminosity AGNs (10(43) ergs(-1) < L0.5-10 keV < 10(44) erg s(-1)) tend to have red colors, while the highest-luminosity AGNs (L0.5-10 keV > 10(45) erg s(-1)) have bluer colors; higher spectroscopic completeness of the Stripe 82X sample is needed to determine whether this is a selection effect or an intrinsic property. Finally, we parameterize X-ray obscuration of Stripe 82X AGNs by calculating their hardness ratios (HRs) and find no clear trends between HR and optical reddening. Our results will help inform best-effort practices in following. up obscured AGN candidates in current and future wide-area, shallow X-ray surveys, including the all-sky eROSITA mission.
C1 [LaMassa, Stephanie M.; Civano, Francesca; Urry, C. Meg; Cales, Sabrina; Natarajan, Priyamvada] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
[LaMassa, Stephanie M.; Urry, C. Meg; Cales, Sabrina; Natarajan, Priyamvada] Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA.
[Civano, Francesca] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Brusa, Marcella] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Brusa, Marcella; Cappelluti, Nico; Comastri, Andrea] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Gallagher, Sarah] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cales, Sabrina; Treister, Ezequiel] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Cardamone, Carolin] Wheelock Coll, Dept Math & Sci, 200 Riverway, Boston, MA 02215 USA.
[Farrah, Duncan] Virginia Polytech Inst & State Univ, Dept Phys MC 0435, 850 West Campus Dr, Blacksburg, VA 24061 USA.
[Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Komossa, S.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Merloni, Andrea; Salvato, Mara] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Mroczkowski, Tony] Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Natarajan, Priyamvada] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
[Richards, Gordon] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Schawinski, Kevin] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
RP LaMassa, SM (reprint author), Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.; LaMassa, SM (reprint author), Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA.
OI Mroczkowski, Tony/0000-0003-3816-5372; Cappelluti,
Nico/0000-0002-1697-186X; Schawinski, Kevin/0000-0001-5464-0888; Urry,
Meg/0000-0002-0745-9792
FU FP7 Career Integration Grant "eEASy" [CIG 321913]; National Research
Council Research Associateship Award at the Naval Research Laboratory;
Swiss National Science Foundation Professorship grant [PP00P2-138979/1];
Center of Excellence in Astrophysics and Associated Technologies [PFB
06]; CONICYT Anillo project [ACT1101]; Alfred P. Sloan Foundation;
National Science Foundation; U.S. Department of Energy; National
Aeronautics and Space Administration; Japanese Monbukagakusho; Max
Planck Society; Higher Education Funding Council for England; U.S.
Department of Energy Office of Science; [NNX15AJ40G]
FX S.M.L. acknowledges support from grant number NNX15AJ40G. M.B.
acknowledges support from the FP7 Career Integration Grant "eEASy" (CIG
321913). Support for T.M. comes from a National Research Council
Research Associateship Award at the Naval Research Laboratory. K.S.
gratefully acknowledges support from Swiss National Science Foundation
Professorship grant PP00P2-138979/1. Support for the work of E.T. was
provided by the Center of Excellence in Astrophysics and Associated
Technologies (PFB 06) and by the CONICYT Anillo project ACT1101.;
Funding for the SDSS and SDSS-II has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, the U.S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England. The SDSS
Web site is http://www.sdss3.org/.; Funding for SDSS-III has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, and the U.S. Department
of Energy Office of Science. The SDSS-III Web site is
http://www.sdss3.org/.; This publication makes use of data products from
the Widefield Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
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PG 16
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SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800088
ER
PT J
AU Li, GJ
Winn, JN
AF Li, Gongjie
Winn, Joshua N.
TI ARE TIDAL EFFECTS RESPONSIBLE FOR EXOPLANETARY SPIN-ORBIT ALIGNMENT?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; planetary systems
ID CLOSE-IN PLANETS; ACCRETING MAGNETIC PROTOSTARS; INTERNAL GRAVITY-WAVES;
HOT JUPITERS; STELLAR ROTATION; INERTIAL WAVES; FLUID BODIES; SYSTEMS;
STARS; MISALIGNMENT
AB The obliquities of planet-hosting stars are clues about the formation of planetary systems. Previous observations led to the hypothesis that for close-in giant planets, spin-orbit alignment is enforced by tidal interactions. Here, we examine two problems with this hypothesis. First, Mazeh and coworkers recently used a new technique-based on the amplitude of starspot-induced photometric variability-to conclude that spin-orbit alignment is common even for relatively long-period planets, which would not be expected if tides were responsible. We re-examine the data and find a statistically significant correlation between photometric variability and planetary orbital period that is qualitatively consistent with tidal interactions. However it is still difficult to explain quantitatively, as it would require tides to be effective for periods as long as tens of days. Second, Rogers and Lin argued against a particular theory for tidal re-alignment by showing that initially retrograde systems would fail to be re-aligned, in contradiction with the observed prevalence of prograde systems. We investigate a simple model that overcomes this problem by taking into account the dissipation of inertial waves and the equilibrium tide, as well as magnetic braking. We identify a region of parameter space where re-alignment can be achieved, but it only works for close-in giant planets, and requires some fine tuning. Thus, while we find both problems to be more nuanced than they first appeared, the tidal model still has serious shortcomings.
C1 [Li, Gongjie] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Winn, Joshua N.] MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
EM gli@cfa.harvard.edu
FU NASA Origins program [NNX11AG85G]
FX The authors thank the anonymous referee for a constructive critique of
the manuscript; Hyung Suk Tak, Kevin Schlaufman and Molei Tao for advice
on the statistical methods; Dong Lai for helpful discussions on the
tidal models; and Smadar Naoz, Konstantin Batygin and Bekki Dawson for
helpful discussions on misalignment mechanisms. G.L. is grateful for the
helpful discussions and lectures at the Summer School in Statistics for
Astronomers XI at the Penn State University. J.N.W. is grateful to the
NASA Origins program for financial support (grant NNX11AG85G).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 5
DI 10.3847/0004-637X/818/1/5
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800005
ER
PT J
AU Mann, AW
Gaidos, E
Mace, GN
Johnson, MC
Bowler, BP
LaCourse, D
Jacobs, TL
Vanderburg, A
Kraus, AL
Kaplan, KF
Jaffe, DT
AF Mann, Andrew W.
Gaidos, Eric
Mace, Gregory N.
Johnson, Marshall C.
Bowler, Brendan P.
LaCourse, Daryll
Jacobs, Thomas L.
Vanderburg, Andrew
Kraus, Adam L.
Kaplan, Kyle F.
Jaffe, Daniel T.
TI ZODIACAL EXOPLANETS IN TIME (ZEIT). I. A NEPTUNE-SIZED PLANET ORBITING
AN M4.5 DWARF IN THE HYADES STAR CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: fundamental parameters; stars: individual
(K2-25) stars; late-type; stars: low-mass; stars: statistics
ID LOW-MASS STARS; DIGITAL SKY SURVEY; INTEGRAL-FIELD SPECTROGRAPH; KEPLER
LIGHT CURVES; TRANSMISSION SPECTRUM; SPECTROSCOPIC SURVEY; TRANSITING
PLANETS; CANDIDATE PLANETS; STELLAR ROTATION; PROPER MOTIONS
AB Studying the properties of young planetary systems can shed light on how the dynamics and structure of planets evolve during their most formative years. Recent K2 observations of nearby young clusters (10-800 Myr) have. facilitated the discovery of such planetary systems. Here we report the discovery of a Neptune-sized planet transiting an M4.5 dwarf (K2-25) in the Hyades cluster (650-800 Myr). The light. curve shows a strong periodic signal at 1.88 days, which we attribute to spot coverage and rotation. We confirm that. the planet host is a member of the Hyades by measuring the radial velocity of the system with the high-resolution near-infrared spectrograph Immersion Grating Infrared Spectrometer. This enables us to calculate a distance based on K2-25's kinematics and membership to the Hyades, which in turn provides a stellar radius and mass to; 5%-10%, better than what is currently possible for most Kepler M dwarfs (12%-20%). We use the derived stellar density as a prior on fitting the K2 transit photometry, which provides weak constraints on eccentricity. Utilizing a combination of adaptive optics imaging and high-resolution spectra, we rule out the possibility that the signal is due to a bound or background eclipsing binary, confirming the transits' planetary origin. K2-25b has a radius (3.43 (+0.95)(-0.31)- R-circle plus) much larger than older Kepler planets with similar orbital periods (3.485 days) and host-star masses (0.29 M-circle dot). This suggests that close-in planets lose some of their atmospheres past the first few hundred million years. Additional transiting planets around the Hyades, Pleiades, and Praesepe clusters from K2 will help confirm whether this planet is atypical or representative of other close-in planets of similar age.
C1 [Mann, Andrew W.; Mace, Gregory N.; Johnson, Marshall C.; Bowler, Brendan P.; Kraus, Adam L.; Kaplan, Kyle F.; Jaffe, Daniel T.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
[Gaidos, Eric] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA.
[Bowler, Brendan P.] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Mann, AW (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM amann@astro.as.utexas.edu
FU Space Telescope Science Institute [51364]; NASA [NAS 5-26555,
NNX11AC33G]; Swiss National Science Foundation; US National Science
Foundation [ASTR1229522]; University of Texas at Austin; Korean GMT
Project of KASI; NASA Office of Space Science [NNX09AF08G]; Robert
Martin Ayers Sciences Fund
FX A.W.M. was supported through Hubble Fellowship grant 51364 awarded by
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., for NASA,
under contract NAS 5-26555. This research was supported by NASA grant
NNX11AC33G to E.G.. E.G. was also supported by an International Visitor
grant from the Swiss National Science Foundation. We thank Bandit for
his useful discussions and encouragement during the writing of this
manuscript.; This work used the Immersion Grating Infrared Spectrograph
(IGRINS), which was developed under a collaboration between the
University of Texas at Austin and the Korea Astronomy and Space Science
Institute (KASI) with the financial support of the US National Science
Foundation under grant ASTR1229522, of the University of Texas at
Austin, and of the Korean GMT Project of KASI. The IGRINS pipeline
package PLP was developed by Dr. Jae-Joon Lee at Korea Astronomy and
Space Science Institute and Professor Soojong Pak's team at Kyung Hee
University. SNIFS on the UH 2.2 m telescope is part of the Nearby
Supernova Factory project, a scientific collaboration among the Centre
de Recherche Astronomique de Lyon, Institut de Physique Nucleaire de
Lyon, Laboratoire de Physique Nucleaire et des Hautes Energies, Lawrence
Berkeley National Laboratory, Yale University, University of Bonn, Max
Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and
the Centre de Physique des Particules de Marseille. Some of the data
presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. Support for MAST for non-HST data is provided by the NASA
Office of Space Science via grant NNX09AF08G and by other grants and
contracts. This research was made possible through the use of the AAVSO
Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers
Sciences Fund. The authors acknowledge the Texas Advanced Computing
Center (TACC) at The University of Texas at Austin for providing grid
resources that have contributed to the research results reported within
this paper.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800046
ER
PT J
AU Safarzadeh, M
Hayward, CC
Ferguson, HC
Somerville, RS
AF Safarzadeh, Mohammadtaher
Hayward, Christopher C.
Ferguson, Henry C.
Somerville, Rachel S.
TI WHAT SHAPES THE FAR-INFRARED SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust; extinction
ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; SMOOTHED
PARTICLE HYDRODYNAMICS; REDSHIFT SUBMILLIMETER GALAXIES;
HERSCHEL-SELECTED GALAXIES; RADIATIVE-TRANSFER; STARBURST GALAXIES;
FORMATION RATES; INTERSTELLAR DUST
AB To explore the connection between the global physical properties of galaxies and their far-infrared (FIR) spectral energy distributions (SEDs), we study the variation in the FIR SEDs of a set of 51 hydrodynamically simulated galaxies, both mergers and isolated systems representative of low-and high-redshift galaxies, that are generated by performing dust radiative transfer in post-processing. We study the FIR SEDs using principal component (PC) analysis, and find that 97% of the variance in the sample can be explained by two PCs. The first PC characterizes the wavelength of the peak of the FIR SED, and the second encodes the breadth of the SED. We find that the coefficients of both PCs can be predicted well using a double power law in terms of the IR luminosity and dust mass, which suggests that these two physical properties are the primary determinants of galaxies' FIR SED shapes. Incorporating galaxy sizes does not significantly improve our ability to predict the FIR SEDs. Our results suggest that the observed redshift evolution in the effective dust temperature at a fixed IR luminosity is not driven by geometry: the SEDs of z similar to 2-3 ultraluminous IR galaxies (ULIRGs) are cooler than those of local ULIRGs, not because the high-redshift galaxies are more extended, but rather because they have higher dust masses at fixed IR luminosity. Finally, based on our simulations, we introduce a two-parameter set of SED templates that depend on both IR luminosity and dust mass.
C1 [Safarzadeh, Mohammadtaher] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, 3400 N Charles St, Baltimore, MD 21218 USA.
[Hayward, Christopher C.] CALTECH, TAPIR 350 17, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Hayward, Christopher C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Ferguson, Henry C.] Space Telescope Sci Inst, 3700 San Martin Blvd, Baltimore, MD 21218 USA.
[Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
RP Safarzadeh, M (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, 3400 N Charles St, Baltimore, MD 21218 USA.
EM mts@pha.jhu.edu
OI Hayward, Christopher/0000-0003-4073-3236
FU Gordon and Betty Moore Foundation; National Science Foundation
[PHY-1066293]; Simons Foundation in the form of a Simons Investigator
Award; NASA's Astrophysics Data Analysis Program [NNX15AE54G]
FX We thank Maarten Baes for comments on the manuscript and Brice Menard
and Nick Scoville for useful discussions. C.C.H. is grateful to the
Gordon and Betty Moore Foundation for financial support. C.C.H. and
R.S.S. acknowledge the hospitality of the Aspen Center for Physics,
which is supported by the National Science Foundation Grant No.
PHY-1066293. R.S.S. is grateful to the Downsbrough family for their
support and acknowledges support from the Simons Foundation in the form
of a Simons Investigator Award. This work was partially supported by
NASA's Astrophysics Data Analysis Program, under grant NNX15AE54G.
NR 107
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800062
ER
PT J
AU Shen, Y
Horne, K
Grier, CJ
Peterson, BM
Denney, KD
Trump, JR
Sun, MY
Brandt, WN
Kochanek, CS
Dawson, KS
Green, PJ
Greene, JE
Hall, PB
Ho, LC
Jiang, LH
Kinemuchi, K
McGreer, ID
Petitjean, P
Richards, GT
Schneider, DP
Strauss, MA
Tao, C
Wood-Vasey, WM
Zu, Y
Pan, KK
Bizyaev, D
Ge, J
Oravetz, D
Simmons, A
AF Shen, Yue
Horne, Keith
Grier, C. J.
Peterson, Bradley M.
Denney, Kelly D.
Trump, Jonathan R.
Sun, Mouyuan
Brandt, W. N.
Kochanek, Christopher S.
Dawson, Kyle S.
Green, Paul J.
Greene, Jenny E.
Hall, Patrick B.
Ho, Luis C.
Jiang, Linhua
Kinemuchi, Karen
McGreer, Ian D.
Petitjean, Patrick
Richards, Gordon T.
Schneider, Donald P.
Strauss, Michael A.
Tao, Charling
Wood-Vasey, W. M.
Zu, Ying
Pan, Kaike
Bizyaev, Dmitry
Ge, Jian
Oravetz, Daniel
Simmons, Audrey
TI THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: FIRST
BROAD-LINE H beta AND Mg II LAGS AT z greater than or similar to 0.3
FROM SIX-MONTH SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; line: profiles; quasars: general;
surveys
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; SEYFERT 1 GALAXIES;
HIGH-LUMINOSITY QUASARS; HIGH ACCRETION RATES; VELOCITY-DELAY MAPS;
SDSS-III; EMISSION-LINES; REGION SIZES; MASS SCALE
AB Reverberation mapping (RM) measurements of broad-line region (BLR) lags in z > 0.3 quasars are important for directly measuring black hole masses in these distant objects, but so far there have been limited attempts and success given the practical difficulties of RM in this regime. Here we report preliminary results of 15 BLR lag measurements from the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project, a dedicated RM program with multi-object spectroscopy designed for RM over a wide redshift range. The lags are based on the 2014 spectroscopic light curves alone (32 epochs over six months) and focus on the H beta and Mg II broad lines in the 100 lowest-redshift (z < 0.8) quasars included in SDSS-RM; they represent a small subset of the lags that SDSS-RM (including 849 quasars to z similar to 4.5) is expected to deliver. The reported preliminary lag measurements are for intermediate-luminosity quasars at 0.3 less than or similar to z < 0.8, including nine H beta lags and six Mg II lags, for the first time extending RM results to this redshift-luminosity regime and providing direct quasar black hole mass estimates over approximately half of cosmic time. The Mg II lags also increase the number of known Mg II lags by several fold. and start to explore the utility of Mg II for RM at high redshift. The location of these new lags at higher redshifts on the observed BLR size-luminosity relationship is statistically consistent with previous H beta results at z < 0.3. However, an independent constraint on the relationship slope at z > 0.3 is not yet possible owing to the limitations in our current sample. Our results demonstrate the general feasibility and potential of multi-object RM for z > 0.3 quasars.
C1 [Shen, Yue] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Shen, Yue] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Shen, Yue] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Horne, Keith] Univ St Andrews, SUPA Phys Astron, St Andrews KY16 9SS, Fife, Scotland.
[Grier, C. J.; Trump, Jonathan R.; Sun, Mouyuan; Brandt, W. N.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Grier, C. J.; Trump, Jonathan R.; Sun, Mouyuan; Brandt, W. N.; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Peterson, Bradley M.; Denney, Kelly D.; Kochanek, Christopher S.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Peterson, Bradley M.; Denney, Kelly D.; Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA.
[Peterson, Bradley M.; Denney, Kelly D.; Kochanek, Christopher S.] Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China.
[Peterson, Bradley M.; Denney, Kelly D.; Kochanek, Christopher S.] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China.
[Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Green, Paul J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Greene, Jenny E.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hall, Patrick B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Ho, Luis C.; Jiang, Linhua] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Ho, Luis C.] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China.
[Kinemuchi, Karen; Pan, Kaike; Bizyaev, Dmitry; Oravetz, Daniel; Simmons, Audrey] Apache Point Observ, POB 59, Sunspot, NM 88349 USA.
[Kinemuchi, Karen; Pan, Kaike; Bizyaev, Dmitry; Oravetz, Daniel; Simmons, Audrey] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA.
[McGreer, Ian D.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Petitjean, Patrick] Univ Paris 06, Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
[Petitjean, Patrick] CNRS, 98bis Blvd Arago, F-75014 Paris, France.
[Richards, Gordon T.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Tao, Charling] Aix Marseille Univ, IN2P3, Ctr Phys Particules Marseille, CNRS, 163 Ave Luminy,Case 902, F-13288 Marseille 09, France.
[Tao, Charling] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China.
[Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Zu, Ying] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
[Ge, Jian] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
RP Shen, Y (reprint author), Univ Illinois, Dept Astron, Urbana, IL 61801 USA.; Shen, Y (reprint author), Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
RI Jiang, Linhua/H-5485-2016
OI Jiang, Linhua/0000-0003-4176-6486
FU NASA [HST-HF-51314, NAS 5-26555, HST-HF-51330]; Space Telescope Science
Institute; UK Science and Technology Facilities Council (STFC)
[ST/M001296/1]; NSF [AST-1517113]; National Science Foundation
[AST-1008882]; NSF AAPF fellowship [AST-1302093]; China Scholarship
Council [[2013] 3009]; Chinese Academy of Science [XDB09030102];
National Natural Science Foundation of China [11473002]; 985 project at
Peking University; V.M. Willaman Endowment; Alfred P. Sloan Foundation;
Participating Institutions; National Science Foundation; U.S. Department
of Energy Office of Science
FX We thank the referee for a careful review and constructive comments.
Support for the work of Y.S. was provided by NASA through Hubble
Fellowship grant number HST-HF-51314, awarded by the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.
K.H. acknowledges support from UK Science and Technology Facilities
Council (STFC) grant ST/M001296/1. C.J.G. and W.N.B. acknowledge support
from NSF grant AST-1517113 and the V.M. Willaman Endowment. B.M.P. is
grateful for support from the National Science Foundation through grant
AST-1008882. K.D.D. is supported by an NSF AAPF fellowship awarded under
NSF grant AST-1302093. J.R.T. acknowledges support from NASA through
Hubble Fellowship grant HST-HF-51330 awarded by the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., for NASA under contract NAS 5-26555.
M.S. acknowledges support from the China Scholarship Council (No. [2013]
3009). L.C.H. is supported by the Chinese Academy of Science through
grant No. XDB09030102 (Emergence of Cosmological Structures) from the
strategic Priority Research Program, and from the National Natural
Science Foundation of China through grant No. 11473002. L.J.
acknowledges the support from a 985 project at Peking University.;
Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III Web site is http://www.sdss3.org/.
NR 62
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
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PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800030
ER
PT J
AU Su, KYL
Rieke, GH
Defrere, D
Wang, KS
Lai, SP
Wilner, DJ
van Lieshout, R
Lee, CF
AF Su, Kate Y. L.
Rieke, George H.
Defrere, Denis
Wang, Kuo-Song
Lai, Shih-Ping
Wilner, David J.
van Lieshout, Rik
Lee, Chin-Fei
TI THE INNER DEBRIS STRUCTURE IN THE FOMALHAUT PLANETARY SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; radio lines: stars; stars:
individual (Fomalhaut)
ID P-R DRAG; KUIPER-BELT; COLLISIONAL EVOLUTION; SIZE DISTRIBUTIONS; SOLAR
CHROMOSPHERE; EXOZODIACAL DUST; EPSILON ERIDANI; HOT DUST; HR 8799; DISK
AB Fomalhaut plays an important role in the study of debris disks and small bodies in other planetary systems. The proximity and luminosity of the star make key features of its debris, like the water ice. line, accessible. Here we present ALMA cycle 1, 870 mu m (345 GHz) observations targeted at the inner part of the Fomalhaut system with a synthesized beam of 0 ''.45 x 0 ''.37 (similar to 3 AU linear resolution at the distance of Fomalhaut) and an rms of 26 mu Jy beam-1. The high angular resolution and sensitivity of the ALMA data enable us to place strong constraints on the nature of the warm excess revealed by Spitzer and Herschel observations. We detect a point source at the star position with a total flux consistent with thermal emission from the stellar photosphere. No structures that are brighter than 3 sigma are detected in the central 15 AU x 15 AU region. Modeling the spectral energy distribution using parameters expected for a dust-producing planetesimal belt indicates a radial location in the range of similar to 8-15 AU. This is consistent with the location where ice sublimates in Fomalhaut, i.e., an asteroid-belt analog. The 3s upper limit for such a belt is <1.3 mJy at 870 mu m. We also interpret the 2 and 8-13 mu m interferometric measurements to reveal the structure in the inner 10 AU region as dust naturally connected to this proposed asteroid belt by Poynting-Robertson drag, dust sublimation, and magnetically trapped nanograins.
C1 [Su, Kate Y. L.; Rieke, George H.; Defrere, Denis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Su, Kate Y. L.; Wang, Kuo-Song; Lai, Shih-Ping; Lee, Chin-Fei] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
[Lai, Shih-Ping] NTHU, Inst Astron, Hsinchu 30013, Taiwan.
[Wilner, David J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[van Lieshout, Rik] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
RP Su, KYL (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.; Su, KYL (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
EM ksu@as.arizona.edu
OI Su, Kate/0000-0002-3532-5580
FU NASA's ADAP program [NNX11AF73G]; NASA [1255094, 1256424]; Ministry of
Science and Technology (MoST) of Taiwan [NSC 98-2112-M-007-007-MY3, NSC
101-2119-M-007-004, MoST 102-2119-M-007-004-MY3]
FX This paper made use of the following ALMA data: ADS/JAO. ALMA
2012.0.00238. S (PI: S.P.L.). ALMA is a partnership of ESO (representing
its member states), NSF (USA), and NINS (Japan), together with NRC
(Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of
Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and
NAOJ. K.Y.L.S. is grateful for funding from NASA's ADAP program (grant
number NNX11AF73G). Support for G.H.R. is provided by NASA through
contract 1255094 and 1256424 issued by JPL/Caltech to the University of
Arizona. S.P.L thanks the support of the Ministry of Science and
Technology (MoST) of Taiwan with Grants NSC 98-2112-M-007-007-MY3, NSC
101-2119-M-007-004, and MoST 102-2119-M-007-004-MY3.
NR 64
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 45
DI 10.3847/0004-637X/818/1/45
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800045
ER
PT J
AU Tobin, JJ
Looney, LW
Li, ZY
Chandler, CJ
Dunham, MM
Segura-Cox, D
Sadavoy, SI
Melis, C
Harris, RJ
Kratter, K
Perez, L
AF Tobin, John J.
Looney, Leslie W.
Li, Zhi-Yun
Chandler, Claire J.
Dunham, Michael M.
Segura-Cox, Dominique
Sadavoy, Sarah I.
Melis, Carl
Harris, Robert J.
Kratter, Kaitlin
Perez, Laura
TI THE VLA NASCENT DISK AND MULTIPLICITY SURVEY OF PERSEUS PROTOSTARS
(VANDAM). II. MULTIPLICITY OF PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; planetary systems; protoplanetary disks; stars:
formation; stars: protostars; techniques: interferometric
ID 1ST HYDROSTATIC CORE; STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; BROWN
DWARF DESERT; IRAM-PDBI SURVEY; SPITZER-SPACE-TELESCOPE; INITIAL MASS
FUNCTION; ORION-NEBULA-CLUSTER; CLOSE BINARY-SYSTEMS; SOLAR-TYPE STARS
AB We present a multiplicity study of all known protostars (94) in the Perseus molecular cloud from a Karl G. Jansky Very Large Array survey at Ka-band (8mm and 1 cm) and C-band (4 and 6.6 cm). The observed sample has a bolometric luminosity range between 0.1 L-circle dot and similar to 33 L-circle dot, with a median of 0.7 L-circle dot. This multiplicity study is based on the Ka-band data, having a best resolution of similar to 0.'' 065 (15 au) and separations out to similar to 43 '' (10,000 au) can be probed. The overall multiplicity fraction (MF) is found to be 0.40 +/- 0.06 and the companion star fraction (CSF) is 0.71 +/- 0.06. The MF and CSF of the Class 0 protostars are 0.57 +/- 0.09 and 1.2 +/- 0.2, and the MF and CSF of Class I protostars are both 0.23 +/- 0.08. The distribution of companion separations appears bi-modal, with a peak at similar to 75 au and another peak at similar to 3000 au. Turbulent fragmentation is likely the dominant mechanism on >1000 au scales and disk fragmentation is likely to be the dominant mechanism on <200 au scales. Toward three Class 0 sources we find companions separated by <30 au. These systems have the smallest separations of currently known Class 0 protostellar binary systems. Moreover, these close systems are embedded within larger (50-400 au) structures and may be candidates for ongoing disk fragmentation.
C1 [Tobin, John J.; Harris, Robert J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Looney, Leslie W.; Segura-Cox, Dominique] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Chandler, Claire J.; Perez, Laura] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
[Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
[Sadavoy, Sarah I.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Kratter, Kaitlin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Tobin, JJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM tobin@strw.leidenuniv.nl
FU Netherlands Organisation for Scientific Research (NWO) [639.041.439];
NASA through Hubble Fellowship [HST-HF-51300.01-A]; Space Telescope
Science Institute; NASA [NAS 5-26555, NNX14AB38G]; Laboratory for
Astronomical Imaging at the University of Illinois; NSF [AST-07-09206];
U.S. National Science Foundation [AST-1313428]; Submillimeter Array
through an SMA postdoctoral fellowship; [NSF1313083]
FX We thank the anonymous referee for constructive suggestions that
improved the quality of the manuscript. The authors wish to thank I.(K.)
Lee, A. Stutz, B. Reipurth, J. Jorgensen, A. Kraus, and L. Tychoniec for
useful discussions regarding this work. J.J.T. is currently supported by
grant 639.041.439 from the Netherlands Organisation for Scientific
Research (NWO). J.J.T. acknowledges past support provided by NASA
through Hubble Fellowship grant #HST-HF-51300.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. L.W.L. acknowledges support from the Laboratory for
Astronomical Imaging at the University of Illinois and the NSF under
grant AST-07-09206. Z.Y.L. is supported in part by NSF1313083 and NASA
NNX14AB38G. C.M. acknowledges financial support from the U.S. National
Science Foundation through award AST-1313428. M.M.D. acknowledges
support from the Submillimeter Array through an SMA postdoctoral
fellowship. This research made use of Astropy, a community-developed
core Python package for Astronomy (Astropy Collaboration, 2013,.
http://www.astropy.org). This research made use of APLpy, an open-source
plotting package for Python hosted at http://aplpy.github.com. This
research has made use of NASA's Astrophysics Data System. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 152
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 73
DI 10.3847/0004-637X/818/1/73
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800073
ER
PT J
AU Toy, VL
Cenko, SB
Silverman, JM
Butler, NR
Cucchiara, A
Watson, AM
Bersier, D
Perley, DA
Margutti, R
Bellm, E
Bloom, JS
Cao, Y
Capone, JI
Clubb, K
Corsi, A
De Cia, A
de Diego, JA
Filippenko, AV
Fox, OD
Gal-Yam, A
Gehrels, N
Georgiev, L
Gonzalez, JJ
Kasliwal, MM
Kelly, PL
Kulkarni, SR
Kutyrev, AS
Lee, WH
Prochaska, JX
Ramirez-Ruiz, E
Richer, MG
Roman-Zuniga, C
Singer, L
Stern, D
Troja, E
Veilleux, S
AF Toy, V. L.
Cenko, S. B.
Silverman, J. M.
Butler, N. R.
Cucchiara, A.
Watson, A. M.
Bersier, D.
Perley, D. A.
Margutti, R.
Bellm, E.
Bloom, J. S.
Cao, Y.
Capone, J. I.
Clubb, K.
Corsi, A.
De Cia, A.
de Diego, J. A.
Filippenko, A. V.
Fox, O. D.
Gal-Yam, A.
Gehrels, N.
Georgiev, L.
Gonzalez, J. J.
Kasliwal, M. M.
Kelly, P. L.
Kulkarni, S. R.
Kutyrev, A. S.
Lee, W. H.
Prochaska, J. X.
Ramirez-Ruiz, E.
Richer, M. G.
Roman-Zuniga, C.
Singer, L.
Stern, D.
Troja, E.
Veilleux, S.
TI OPTICAL AND NEAR-INFRARED OBSERVATIONS OF SN 2013DX ASSOCIATED WITH GRB
130702A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 130702A); supernovae: individual (SN
2013dx)
ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; 25 APRIL 1998; LATE-TIME
SPECTRA; LIGHT CURVES; IC SUPERNOVAE; RELATIVISTIC SUPERNOVAE; BRIGHT
SUPERNOVA; LOW-RESOLUTION; IA SUPERNOVAE
AB We present optical and near-infrared (NIR) light curves and optical spectra of SN 2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB 130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is measured to be E gamma,iso = 6.4(-1.0)(+1.3) x 10(50) erg (1 keV to 10 MeV in the rest frame), placing it intermediate between low-luminosity GRBs like GRB 980425/SN 1998bw and the broader cosmological population. We compare the observed g'r'i'z' light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves similar to 20% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined SNe Ic, both associated with (SN 2006aj and SN 1998bw) and lacking (SN 1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric velocities around peak of similar to 21,000 km s(-1). We construct a quasi-bolometric (g'r'i'z'yJ) light curve for SN 2013dx, only the fifth GRB-associated SN with extensive NIR coverage and the third with a bolometric light curve extending beyond Delta t > 40 days. Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a Ni-56 mass of M-Ni = 0.37 +/- 0.01 M-circle dot, an ejecta mass of M-ej = 3.1 +/- 0.1 M-circle dot, and a kinetic energy of E-K = (8.2 +/- 0.43) x 10(51) erg (statistical uncertainties only), consistent with previous GRB-associated supernovae. When considering the ensemble population of GRB-associated supernovae, we find no correlation between the mass of synthesized Ni-56 and high-energy properties, despite clear predictions from numerical simulations that M-Ni should correlate with the degree of asymmetry. On the other hand, M-Ni clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.
C1 [Toy, V. L.; Capone, J. I.; Troja, E.; Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cenko, S. B.; Cucchiara, A.; Gehrels, N.; Kutyrev, A. S.; Singer, L.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cenko, S. B.; Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Silverman, J. M.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
[Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Watson, A. M.; de Diego, J. A.; Georgiev, L.; Gonzalez, J. J.; Lee, W. H.; Richer, M. G.; Roman-Zuniga, C.] Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 106, Ensenada 22800, Baja California, Mexico.
[Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Perley, D. A.; Bellm, E.; Cao, Y.; Kulkarni, S. R.] CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Margutti, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bloom, J. S.; Clubb, K.; Filippenko, A. V.; Fox, O. D.; Kelly, P. L.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Corsi, A.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA.
[De Cia, A.; Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel.
[Kasliwal, M. M.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Prochaska, J. X.; Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA.
[Singer, L.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Toy, VL (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Roman-Zuniga, Carlos/F-6602-2016; Gonzalez, Jose/L-6687-2014;
OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Gonzalez,
Jose/0000-0002-3724-1583; Bellm, Eric/0000-0001-8018-5348
FU NASA; NSF; Alfred P. Sloan Foundation; U.S. Department of Energy Office
of Science
FX This research has made use of the VizieR catalog access tool, CDS,
Strasbourg, France. This publication also uses data products from the
Two Micron All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by NASA and the NSF. Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the NSF, and the U.S. Department of Energy
Office of Science. The SDSS-III website is http://www.sdss3.org/.
SDSS-III is managed by the Astrophysical Research Consortium for the
Participating Institutions of the SDSS-III Collaboration including the
University of Arizona, the Brazilian Participation Group, Brookhaven
National Laboratory, Carnegie Mellon University, University of Florida,
the French Participation Group, the German Participation Group, Harvard
University, the Instituto de Astrofisica de Canarias, the Michigan
State/Notre Dame/JINA Participation Group, Johns Hopkins University,
Lawrence Berkeley National Laboratory, Max Planck Institute for
Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University.
NR 148
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 79
DI 10.3847/0004-637X/818/1/79
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800079
ER
PT J
AU Wittenmyer, RA
Johnson, JA
Butler, RP
Horner, J
Wang, L
Robertson, P
Jones, MI
Jenkins, JS
Brahm, R
Tinney, CG
Mengel, MW
Clark, J
AF Wittenmyer, Robert A.
Johnson, John Asher
Butler, R. P.
Horner, Jonathan
Wang, Liang
Robertson, Paul
Jones, M. I.
Jenkins, J. S.
Brahm, R.
Tinney, C. G.
Mengel, M. W.
Clark, J.
TI THE PAN-PACIFIC PLANET SEARCH. IV. TWO SUPER-JUPITERS IN A 3:5 RESONANCE
ORBITING THE GIANT STAR HD 33844
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HD 33844); techniques: radial
velocities
ID ANGLO-AUSTRALIAN PLANET; PRECISE RADIAL-VELOCITIES; POST-MS EVOLUTION;
2-PLANET SYSTEMS; DETECTION LIMITS; PERIOD PLANETS; BROWN DWARF;
METAL-RICH; MASS STARS; HOST STAR
AB We report the discovery of two giant planets orbiting the K giant HD 33844 based on radial velocity data from three independent campaigns. The planets move on nearly circular orbits with semimajor axes a(b) = 1.60 +/- 0.02 AU and a(c) = 2.24 +/- 0.05 AU, and have minimum masses (m sin i) of M-b = 1.96 +/- 0.12 M-Jup and M-c = 1.76 +/- 0.18 M-Jup. Detailed N- body dynamical simulations show that the two planets have remained on stable orbits for more than 10(6) years for low eccentricities and are most likely trapped in a mutual 3:5 mean motion resonance.
C1 [Wittenmyer, Robert A.; Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Wittenmyer, Robert A.; Horner, Jonathan; Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Wittenmyer, Robert A.; Horner, Jonathan; Mengel, M. W.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia.
[Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Wang, Liang] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China.
[Robertson, Paul] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Robertson, Paul] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Jones, M. I.] Pontificia Univ Catolica Chile, Dept Elect Engn, Ave Vicua Mackenna 4860, Santiago 7820436, Chile.
[Jones, M. I.] Pontificia Univ Catolica Chile, Ctr Astroengn UC, Ave Vicua Mackenna 4860, Santiago 7820436, Chile.
[Jenkins, J. S.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[Brahm, R.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Brahm, R.] Millennium Inst Astrophys, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Clark, J.] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia.
RP Wittenmyer, RA (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.; Wittenmyer, RA (reprint author), Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.; Wittenmyer, RA (reprint author), Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia.
EM rob@unsw.edu.au
RI Jenkins, James/I-5284-2016; Butler, Robert/B-1125-2009;
OI Mengel, Matthew/0000-0002-7830-6822; Tinney,
Christopher/0000-0002-7595-0970; Wang, Liang/0000-0003-3603-1901;
Horner, Jonti/0000-0002-1160-7970
FU USQ's Strategic Research Fund: the STARWINDS project; Australian
Research Council [DP0774000, DP130102695]
FX J.H. is supported by USQ's Strategic Research Fund: the STARWINDS
project. C.G.T. is supported by Australian Research Council grants
DP0774000 and DP130102695. We gratefully acknowledge the efforts of PPPS
guest observers Brad Carter, Hugh Jones, and Simon O'Toole. This
research has made use of NASA's Astrophysics Data System (ADS) and the
SIMBAD database operated at CDS, Strasbourg, France. This research has
also made use of the Exoplanet Orbit Database and the Exoplanet Data
Explorer at exoplanets.org (Wright et al. 2011).
NR 75
TC 1
Z9 1
U1 2
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2016
VL 818
IS 1
AR 35
DI 10.3847/0004-637X/818/1/35
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE1EZ
UT WOS:000370370800035
ER
PT J
AU Zhang, K
Bergin, EA
Blake, GA
Cleeves, LI
Hogerheijde, M
Salinas, V
Schwarz, KR
AF Zhang, Ke
Bergin, Edwin A.
Blake, Geoffrey A.
Cleeves, L. Ilsedore
Hogerheijde, Michiel
Salinas, Vachail
Schwarz, Kamber R.
TI y ON THE COMMONALITY OF 10-30AU SIZED AXISYMMETRIC DUST STRUCTURES IN
PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE protoplanetary disks; stars: pre-main sequence; techniques:
interferometric
ID TRANSITIONAL DISKS; PLANET FORMATION; SNOW LINE; HL TAURI; GAS;
PLANETESIMALS; TURBULENCE; SOLIDS; FLOWS; SOLAR
AB An unsolved problem in step-wise core-accretion planet formation is that rapid radial drift in gas-rich protoplanetary disks should drive millimeter-/meter-sized particles inward to the central star before large bodies can form. One promising solution is to confine solids within small-scale structures. Here, we investigate dust structures in the (sub) millimeter. continuum emission of four disks (TW Hya, HL Tau, HD 163296, and DM Tau), a sample of disks with the highest spatial resolution Atacama Large Millimeter/submillimeter Array observations to date. We retrieve the surface brightness distributions using synthesized images and fitting visibilities with analytical functions. We find that the continuum emission of the four disks is similar to axisymmetric but rich in 10-30 AU-sized radial structures, possibly due to physical gaps, surface density enhancements, or localized dust opacity variations within the disks. These results suggest that small-scale axisymmetric dust structures are likely to be common, as a result of ubiquitous processes in disk evolution and planet formation. Compared with recent spatially resolved observations of CO snow. lines in these same disks, all four systems show enhanced continuum emission from regions just beyond the CO condensation fronts, potentially suggesting a causal relationship between dust growth/trapping and snow. lines.
C1 [Zhang, Ke; Bergin, Edwin A.; Schwarz, Kamber R.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA.
[Cleeves, L. Ilsedore] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Hogerheijde, Michiel; Salinas, Vachail] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Zhang, K (reprint author), Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
EM kezhang@umich.edu
RI zhang, ke/A-3898-2009
OI zhang, ke/0000-0002-0661-7517
FU National Science Foundation (INSPIRE) [AST-1344133, AST-1514670]
FX This work was supported by funding from the National Science Foundation,
grants AST-1344133 (INSPIRE) and AST-1514670. The authors thank John
Monnier for discussions on model-fitting approaches to visibility data.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc., This paper makes use of the following ALMA data
sets: ADS/JAO. ALMA#2011.0.00015.SV, ADS/JAO. ALMA#2013.1.00198.S and
ADS/JAO. ALMA #2013.1.01268.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ.
NR 39
TC 14
Z9 14
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2016
VL 818
IS 1
AR L16
DI 10.3847/2041-8205/818/1/L16
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD0JG
UT WOS:000369605600016
ER
PT J
AU Labandeira, CC
Yang, Q
Santiago-Blay, JA
Hotton, CL
Monteiro, A
Wang, YJ
Goreva, Y
Shih, CK
Siljestrom, S
Rose, TR
Dilcher, DL
Ren, D
AF Labandeira, Conrad C.
Yang, Qiang
Santiago-Blay, Jorge A.
Hotton, Carol L.
Monteiro, Antonia
Wang, Yong-Jie
Goreva, Yulia
Shih, ChungKun
Siljestrom, Sandra
Rose, Tim R.
Dilcher, David L.
Ren, Dong
TI The evolutionary convergence of mid-Mesozoic lacewings and Cenozoic
butterflies
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE angiosperms; gymnosperms; Kalligrammatidae; Papilionoidea; tubular
proboscis; wing eyespots
ID YIXIAN FORMATION; NEUROPTERIDA INSECTA; POLLINATION; KALLIGRAMMATIDAE;
GYMNOSPERMS; CHINA; EYESPOTS; AMERICA; MIMICRY; MELANIN
AB Mid-Mesozoic kalligrammatid lacewings (Neuroptera) entered the fossil record 165 million years ago (Ma) and disappeared 45 Ma later. Extant papilionoid butterflies (Lepidoptera) probably originated 80-70 Ma, long after kalligrammatids became extinct. Although poor preservation of kalligrammatid fossils previously prevented their detailed morphological and ecological characterization, we examine new, well-preserved, kalligrammatid fossils from Middle Jurassic and Early Cretaceous sites in northeastern China to unravel a surprising array of similar morphological and ecological features in these two, unrelated clades. We used polarized light and epifluorescence photography, SEM imaging, energy dispersive spectrometry and time-of-flight secondary ion mass spectrometry to examine kalligrammatid fossils and their environment. We mapped the evolution of specific traits onto a kalligrammatid phylogeny and discovered that these extinct lacewings convergently evolved wing eyespots that possibly contained melanin, and wing scales, elongate tubular proboscides, similar feeding styles, and seed-plant associations, similar to butterflies. Long-proboscid kalligrammatid lacewings lived in ecosystems with gymnosperm-insect relationships and likely accessed bennettitalean pollination drops and pollen. This system later was replaced by mid-Cretaceous angiosperms and their insect pollinators.
C1 [Labandeira, Conrad C.; Yang, Qiang; Wang, Yong-Jie; Shih, ChungKun; Ren, Dong] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China.
[Labandeira, Conrad C.; Santiago-Blay, Jorge A.; Hotton, Carol L.; Shih, ChungKun] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Goreva, Yulia; Siljestrom, Sandra; Rose, Tim R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA.
[Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA.
[Yang, Qiang] Sun Yat Sen Univ, Sch Life Sci, Coll Ecol & Evolut,Guangdong Higher Educ Inst, State Key Lab Biocontrol,Key Lab Biodivers Dynam, Guangzhou 510275, Guangdong, Peoples R China.
[Yang, Qiang] Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China.
[Santiago-Blay, Jorge A.] Univ Puerto Rico, Dept Crop & Agroenvironm Sci, Mayaguez, PR 00681 USA.
[Hotton, Carol L.] Natl Lib Med, Natl Ctr Biotechnol Informat, Bethesda, MD 20892 USA.
[Monteiro, Antonia] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06511 USA.
[Monteiro, Antonia] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore.
[Monteiro, Antonia] Yale NUS Coll, Singapore 138614, Singapore.
[Goreva, Yulia] CALTECH, Jet Prop Lab, Natl Aeronaut & Space Adm, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Siljestrom, Sandra] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, S-51115 Boras, Sweden.
[Siljestrom, Sandra] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Dilcher, David L.] Indiana Univ, Dept Geol, Bloomington, IN 47405 USA.
[Dilcher, David L.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA.
RP Labandeira, CC; Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China.; Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.; Labandeira, CC (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.; Labandeira, CC (reprint author), Univ Maryland, BEES Program, College Pk, MD 20742 USA.
EM labandec@si.edu; rendong@mail.cnu.edu.cn
OI Monteiro, Antonia/0000-0001-9696-459X
FU National Basic Research Program of China (973 Program) [2012CB821906];
National Science Foundation of China [31230065, 31309105, 31372243,
41272006, 41372013]; Beijing Municipal Commission of Education Project
[201207120]; China Postdoctoral Science Foundation [2012T50113];
Doctoral Program of Higher Education of China [20131108120005]; Beijing
Natural Science Foundation [5132008]; Great Wall Scholar Project of the
Beijing Municipal Commission of Education [KZ201310028033]; Program for
Changjiang Scholars and Innovative Research Teams at University
[IRT13081]; Natural Science Foundation of Hebei Province [C2015403012];
Intramural Research Program of the National Institutes of Health,
Library of Medicine; Deep Carbon Observatory; Postdoctoral Fellowship
Program of the Geophysical Laboratory, Carnegie Institution of
Washington; Swedish National Space Board [121/11]
FX This work was supported by the National Basic Research Program of China
(973 Program) (grant 2012CB821906), National Science Foundation of China
(grant nos. 31230065, 31309105, 31372243, 41272006 and 41372013),
Beijing Municipal Commission of Education Project (grant no. 201207120),
China Postdoctoral Science Foundation (grant no. 2012T50113), Doctoral
Program of Higher Education of China (grant no. 20131108120005), Beijing
Natural Science Foundation (grant 5132008), Great Wall Scholar Project
of the Beijing Municipal Commission of Education (grant no.
KZ201310028033), Program for Changjiang Scholars and Innovative Research
Teams at University (IRT13081), Natural Science Foundation of Hebei
Province (grant no. C2015403012), Intramural Research Program of the
National Institutes of Health, Library of Medicine, to C.L.H. and the
Deep Carbon Observatory to Y.G. and S.S. S.S. also was supported through
the Postdoctoral Fellowship Program of the Geophysical Laboratory,
Carnegie Institution of Washington and the Swedish National Space Board
(contract 121/11).
NR 65
TC 6
Z9 7
U1 6
U2 22
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD FEB 10
PY 2016
VL 283
IS 1824
AR 20152893
DI 10.1098/rspb.2015.2893
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DD5PE
UT WOS:000369975500024
ER
PT J
AU Julca-Canto, M
Aguilar-Perez, MM
Rios, N
Sousa, JPB
Cubilla-Rios, L
AF Julca-Canto, Maria
Aguilar-Perez, Madelaine M.
Rios, Nivia
Sousa, Joao Paulo B.
Cubilla-Rios, Luis
TI Additional new natural products produced by Lentinus strigellus: a
biotechnological approach
SO TETRAHEDRON LETTERS
LA English
DT Article
DE Lentinus strigellus; Anti-parasitic activity; Benzopyran; Biotechnology;
Isopanepoxydone
ID PANEPOXYDONE; STRIGOSUS
AB Lentinus strigellus is an edible macrofungus, which has been suggested to have medicinal uses. We report the isolation and structure elucidation of four new natural products 1-3 and 5 from L strigellus cultured on Sabouraud dextrose agar, using CaCl2 as an elicitor and a pH of 4.6; the culture was incubated at 26 degrees C for 15 days. We also report the first isolation of compound 4 from a fungus. These chemical structures were determined by extensive spectroscopic analyses. Compounds 1-4 are benzopyran derivatives and 5 belongs to the isopanepoxydone family. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Julca-Canto, Maria; Aguilar-Perez, Madelaine M.; Sousa, Joao Paulo B.; Cubilla-Rios, Luis] Univ Panama, Lab Trop Bioorgan Chem, Fac Nat Exact Sci & Technol, Panama City, Panama.
[Rios, Nivia] Univ Panama, Dept Microbiol, Fac Nat Exact Sci & Technol, Panama City, Panama.
[Aguilar-Perez, Madelaine M.; Sousa, Joao Paulo B.; Cubilla-Rios, Luis] Smithsonian Trop Res Inst, Unit 0948, Apo Aa 340020948, Panama.
RP Cubilla-Rios, L (reprint author), Univ Panama, Lab Trop Bioorgan Chem, Fac Nat Exact Sci & Technol, Panama City, Panama.; Cubilla-Rios, L (reprint author), Smithsonian Trop Res Inst, Unit 0948, Apo Aa 340020948, Panama.
EM luis.cubilla@up.ac.pa
FU SENACYT - Panama [COL10-060, FID11-051]; Project of Nagoya Protocols'
Application in Panama
FX This work was supported by grants from SENACYT - Panama (COL10-060 and
FID11-051) and from the Project of Nagoya Protocols' Application in
Panama. We also give our thanks to the personnel of Panama's Ministry of
Environment for their assistance in conducting this research project.
Special thanks to M. Piepenbring and T. Hoffman for the taxonomy of L.
striguellus.
NR 17
TC 0
Z9 0
U1 2
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0040-4039
J9 TETRAHEDRON LETT
JI Tetrahedron Lett.
PD FEB 10
PY 2016
VL 57
IS 6
BP 650
EP 653
DI 10.1016/j.tetlet.2015.12.104
PG 4
WC Chemistry, Organic
SC Chemistry
GA DC4PW
UT WOS:000369203800005
ER
PT J
AU Wilkinson, GS
Carter, GG
Bohn, KM
Adams, DM
AF Wilkinson, Gerald S.
Carter, Gerald G.
Bohn, Kirsten M.
Adams, Danielle M.
TI Non-kin cooperation in bats
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Review
DE by-product mutualism; group augmentation; partner choice; reciprocity;
vampire bats; spear-nosed bats
ID SPEAR-NOSED BATS; COMMON VAMPIRE BAT; FEMALE BECHSTEINS BATS;
PHYLLOSTOMUS-HASTATUS; INFORMATION-TRANSFER; DESMODUS-ROTUNDUS; SOCIAL
CALLS; ARTIBEUS-JAMAICENSIS; REPRODUCTIVE SUCCESS; RECIPROCAL ALTRUISM
AB Many bats are extremely social. In some cases, individuals remain together for years or even decades and engage in mutually beneficial behaviours among non-related individuals. Here, we summarize ways in which unrelated bats cooperate while roosting, foraging, feeding or caring for offspring. For each situation, we ask if cooperation involves an investment, and if so, what mechanisms might ensure a return. While some cooperative outcomes are likely a by-product of selfish behaviour as they are in many other vertebrates, we explain how cooperative investments can occur in several situations and are particularly evident in food sharing among common vampire bats (Desmodus rotundus) and alloparental care by greater spear-nosed bats (Phyllostomus hastatus). Fieldwork and experiments on vampire bats indicate that sharing blood with non-kin expands the number of possible donors beyond kin and promotes reciprocal help by strengthening long-term social bonds. Similarly, more than 25 years of recapture data and field observations of greater spearnosed bats reveal multiple cooperative investments occurring within stable groups of non-kin. These studies illustrate how bats can serve as models for understanding how cooperation is regulated in social vertebrates.
C1 [Wilkinson, Gerald S.; Adams, Danielle M.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Carter, Gerald G.] Smithsonian Trop Res Inst, Panama City, Panama.
[Bohn, Kirsten M.] Johns Hopkins Univ, Dept Psychol & Brain Sci, Baltimore, MD 21218 USA.
RP Wilkinson, GS (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
EM wilkinso@umd.edu
OI Wilkinson, Gerald/0000-0001-7799-8444
FU National Science Foundation [IOS-0308642, IOS-1311336]; Ford Foundation
of the National Academy of Sciences; Animal Behavior Society; Society
for the Study of Evolution; American Society of Mammalogists
FX We thank Jack Bradbury, Christina Riehl, Bill Wcislo and an anonymous
reviewer for comments on the manuscript. Our recent work on cooperation
in bats has been supported by the National Science Foundation
(IOS-0308642 and IOS-1311336), the Ford Foundation of the National
Academy of Sciences, the Animal Behavior Society, the Society for the
Study of Evolution and the American Society of Mammalogists.
NR 115
TC 6
Z9 6
U1 34
U2 108
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD FEB 5
PY 2016
VL 371
IS 1687
AR 20150095
DI 10.1098/rstb.2015.0095
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA DA0FZ
UT WOS:000367474300012
PM 26729934
ER
PT J
AU Camargo, F
Whalen, JD
Ding, R
Sadeghpour, HR
Yoshida, S
Burgdorfer, J
Dunning, FB
Killian, TC
AF Camargo, F.
Whalen, J. D.
Ding, R.
Sadeghpour, H. R.
Yoshida, S.
Burgdoerfer, J.
Dunning, F. B.
Killian, T. C.
TI Lifetimes of ultra-long-range strontium Rydberg molecules
SO PHYSICAL REVIEW A
LA English
DT Article
AB The lifetimes of the lower-lying vibrational states of ultra-long-range strontium Rydberg molecules comprising one ground-state (5)s(2) S-1(0) atom and one Rydberg atom in the 5s38s(3) S-1 state are reported. The molecules are created in an ultracold gas held in an optical dipole trap and their numbers determined using field ionization, the product electrons being detected by a microchannel plate. The measurements show that, in marked contrast to earliermeasurements involving rubidium Rydberg molecules, the lifetimes of the low-lying molecular vibrational states are very similar to those of the parent Rydberg atoms. This results because the strong p-wave resonance in low-energy electron-rubidium scattering, which strongly influences the rubidium molecular lifetimes, is not present for strontium. The absence of this resonance offers advantages for experiments involving strontium Rydberg atoms as impurities in quantum gases and for testing of theories of molecular formation and decay.
C1 [Camargo, F.; Whalen, J. D.; Ding, R.; Dunning, F. B.; Killian, T. C.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
[Yoshida, S.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
RP Camargo, F (reprint author), Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
EM Francisco.Camargo@Rice.edu
FU AFOSR [FA9550-14-1-0007]; NSF [1301773, 1205946]; Robert A. Welch
Foundation [C-0734, C-1844]; FWF (Austria) [P23359-N16, FWF-SFB049]
FX This research was supported by the AFOSR under Grant No.
FA9550-14-1-0007, the NSF under Grants No. 1301773 and No. 1205946, the
Robert A. Welch Foundation under Grants No. C-0734 and No. C-1844, the
FWF (Austria) under Grant No. P23359-N16, and FWF-SFB049 NextLite. The
Vienna scientific cluster was used for the calculations. H.R.S. was
supported by a grant to ITAMP from the NSF.
NR 21
TC 4
Z9 4
U1 1
U2 8
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD FEB 4
PY 2016
VL 93
IS 2
AR 022702
DI 10.1103/PhysRevA.93.022702
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DC6ZH
UT WOS:000369367600005
ER
PT J
AU Suosaari, EP
Reid, RP
Playford, PE
Foster, JS
Stolz, JF
Casaburi, G
Hagan, PD
Chirayath, V
Macintyre, IG
Planavsky, NJ
Eberli, GP
AF Suosaari, E. P.
Reid, R. P.
Playford, P. E.
Foster, J. S.
Stolz, J. F.
Casaburi, G.
Hagan, P. D.
Chirayath, V.
Macintyre, I. G.
Planavsky, N. J.
Eberli, G. P.
TI New multi-scale perspectives on the stromatolites of Shark Bay, Western
Australia
SO SCIENTIFIC REPORTS
LA English
DT Article
ID MODERN MARINE STROMATOLITES; MICROBIAL COMMUNITIES; HIGHBORNE CAY; WATER
DEPTH; DIVERSITY; ALIGNMENTS; DATABASE; BAHAMAS; IMAGERY; MATS
AB A recent field-intensive program in Shark Bay, Western Australia provides new multi-scale perspectives on the world's most extensive modern stromatolite system. Mapping revealed a unique geographic distribution of morphologically distinct stromatolite structures, many of them previously undocumented. These distinctive structures combined with characteristic shelf physiography define eight `Stromatolite Provinces'. Morphological and molecular studies of microbial mat composition resulted in a revised growth model where coccoid cyanobacteria predominate in mat communities forming lithified discrete stromatolite buildups. This contradicts traditional views that stromatolites with the best lamination in Hamelin Pool are formed by filamentous cyanobacterial mats. Finally, analysis of internal fabrics of stromatolites revealed pervasive precipitation of microcrystalline carbonate (i.e. micrite) in microbial mats forming framework and cement that may be analogous to the micritic microstructures typical of Precambrian stromatolites. These discoveries represent fundamental advances in our knowledge of the Shark Bay microbial system, laying a foundation for detailed studies of stromatolite morphogenesis that will advance our understanding of benthic ecosystems on the early Earth.
C1 [Suosaari, E. P.; Reid, R. P.; Hagan, P. D.; Eberli, G. P.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33158 USA.
[Suosaari, E. P.] Bush Heritage Australia, Melbourne, Vic 3000, Australia.
[Playford, P. E.] Geol Survey Western Australia, Perth, WA 6004, Australia.
[Foster, J. S.; Casaburi, G.] Univ Florida, Space Life Sci Lab, Dept Microbiol & Cell Sci, Merritt Isl, FL 32953 USA.
[Stolz, J. F.] Duquesne Univ, Dept Biol Sci, Pittsburgh, PA 15282 USA.
[Chirayath, V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Macintyre, I. G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Planavsky, N. J.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA.
RP Reid, RP (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33158 USA.
EM preid@rsmas.miami.edu
FU Chevron; BP; Repsol; Shell; NASA Astrobiology: Exobiology and
Evolutionary Biology program [NNX14AK14G]; NASA Ames Earth Sciences and
Earth Exchange
FX We thank the Geological Survey of Western Australia and Hamelin Station
for logistical support; J. Huff, B. Keyes, J. Mobberley, C. Khodadad, R.
Instrella, A. Shaber-Twedt, and the University of Miami field team for
field and technical assistance; G. Izuno for aerial photos; and the
Western Australian Department of Parks and Wildlife (formerly Department
of Environment and Conservation) and the federal Department of
Sustainability, Environment, Population and Communities for field access
and sampling permits. This project was funded by Chevron, BP, Repsol and
Shell, with additional support from the NASA Astrobiology: Exobiology
and Evolutionary Biology program (NNX14AK14G). Stanford University
Aerospace Design Lab provided flight hardware; NASA Ames Earth Sciences
and Earth Exchange provided support and supercomputer facilities for
image processing. Hamelin Stromatolite Contribution Series #1.
NR 52
TC 5
Z9 5
U1 14
U2 28
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD FEB 3
PY 2016
VL 6
AR 20557
DI 10.1038/srep20557
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC3YZ
UT WOS:000369157800001
PM 26838605
ER
PT J
AU Gross, A
Turner, BL
Goren, T
Berry, A
Angert, A
AF Gross, A.
Turner, B. L.
Goren, T.
Berry, A.
Angert, A.
TI Tracing the Sources of Atmospheric Phosphorus Deposition to a Tropical
Rain Forest in Panama Using Stable Oxygen Isotopes
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID SAHARAN DUST; PHOSPHATES; VARIABILITY; NUTRIENTS; SOILS
AB Atmospheric dust deposition can be a significant source of phosphorus (P) in some tropical forests, so information on the origins and solubility of atmospheric P is needed to understand and predict patterns of forest productivity under future climate scenarios. We characterized atmospheric dust P across a seasonal cycle in a tropical lowland rain forest on Barro Colorado Nature Monument (BCNM), Republic of Panama. We traced P sources by combining remote sensing imagery with the first measurements of stable oxygen isotopes in soluble inorganic phosphate (delta O-18(p)) in dust. In addition, we measured soluble inorganic and organic P concentrations in fine (<1 mu m) and coarse (>1 mu m) aerosol fractions and used this data to estimate the contribution of P inputs from dust deposition to the forest P budget. Aerosol dry mass was greater in the dry season (December to April, 5.6-15.7 mu g m(-3)) than the wet season (May to November, 3.1-7.1 mu g m(-3)). In contrast, soluble P concentrations in the aerosols were lower in the dry season (980-1880 mu g P g(-1)) than the wet season (1170-3380 mu g P g(-1)). The delta O-18(p) of dry-season aerosols resembled that of nearby forest soils (similar to 19.5 parts per thousand), suggesting a local origin. In the wet season, when the Trans-Atlantic Saharan dust belt moves north close to Panama, the delta O-18(p) of aerosols was considerably lower (similar to 15.5 parts per thousand), suggesting a significant contribution of long-distance dust P transport. Using satellite retrieved aerosol optical depth (AOD) and the P concentrations in aerosols we sampled in periods when Saharan dust was evident we estimate that the monthly P input from long distance dust transport during the period with highest Saharan dust deposition is 88 +/- 31 g P ha(-1) month(-1), equivalent to between 10 and 29% of the Pin monthly litter fall in nearby forests. These findings have important implications for our understanding of modern nutrient budgets and the productivity of tropical forests in the region under future climate scenarios.
C1 [Gross, A.; Goren, T.; Berry, A.; Angert, A.] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91905 Jerusalem, Israel.
[Turner, B. L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Goren, T.] Univ Leipzig, Inst Meteorol, D-04109 Leipzig, Germany.
RP Gross, A (reprint author), Hebrew Univ Jerusalem, Inst Earth Sci, IL-91905 Jerusalem, Israel.
EM avner.gross@gmail.com
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
FU Israel Science Foundation [45/14]; GIF, the German-Israeli Foundation
for Scientific Research [1139/2011]; Israel Ministry of Science and
Technology (MOST)
FX This research was supported by a Grant from the Israel Science
Foundation (#45/14) and by a Grant from the GIF, the German-Israeli
Foundation for Scientific Research (#1139/2011). A.G. was funded by the
Israel Ministry of Science and Technology (MOST). We thank Joe Wright
and Raul Rios from the Smithsonian Tropical Research Institute and
Edward Gryspeerdt from Universitat Leipzig for their contribution.
NR 33
TC 2
Z9 2
U1 9
U2 27
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD FEB 2
PY 2016
VL 50
IS 3
BP 1147
EP 1156
DI 10.1021/acs.est.5b04936
PG 10
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DC8LO
UT WOS:000369471300009
PM 26709492
ER
PT J
AU Ward, PS
Blaimer, BB
Fisher, BL
AF Ward, Philip S.
Blaimer, Bonnie B.
Fisher, Brian L.
TI A revised phylogenetic classification of the ant subfamily Formicinae
(Hymenoptera: Formicidae), with resurrection of the genera Colobopsis
and Dinomyrmex
SO ZOOTAXA
LA English
DT Article
DE ant taxonomy; phylogenomics; morphology; convergence; divergence;
Camponotus
ID DIVERSIFICATION; GENUS; EVOLUTION; DIVERSITY; TAXONOMY; ECOLOGY; TREE
AB The classification of the ant subfamily Formicinae is revised to reflect findings from a recent molecular phylogenetic study and complementary morphological investigations. The existing classification is maintained as far as possible, but some tribes and genera are redefined to ensure monophyly. Eleven tribes are recognized, all of which are strongly supported as monophyletic groups: Camponotini, Formicini, Gesomyrmecini, Gigantiopini, Lasiini (= Prenolepidii syn. n.), Melophorini (= Myrmecorhynchini syn.n.; = Notostigmatini syn.n.), Myrmelachistini stat. rev. (= Brachymyrmicini syn. n.), Myrmoteratini, Oecophyllini, Plagiolepidini, and Santschiellini stat. rev. Most of the tribes remain similar in content, but the generic composition of Lasiini, Melophorini, and Plagiolepidini is changed substantially. Species that have been placed in the genus Camponotus belong to three separate lineages. To ensure monophyly of this large, cosmopolitan genus we institute the following changes: Colobopsis and Dinomyrmex, both former subgenera of Camponotus, are elevated to genus level (stat. rev.), and two former genera, Forelophilus and Phasmomyrmex, are demoted to subgenus status (stat. n. and stat. rev., respectively) under Camponotus; two erstwhile subgenera of Phasmomyrmex, Myrmorhachis and Myrmacantha, become junior synonyms (syn.n.) of Camponotus (Phasmomyrmex); and the Camponotus subgenus Myrmogonia becomes a junior synonym (syn.n.) of Colobopsis. Dinomyrmex, represented by a single species from southeast Asia, D. gigas, is quite distinctive, but Camponotus and Colobopsis exhibit more subtle differences, despite being well separated phylogenetically. We identify morphological features of the worker caste that are broadly useful for distinguishing these two genera. Colobopsis species on the islands of New Caledonia and Fiji-regions with few native Camponotus speciestend to exceed these diagnostic bounds, but in this case regionally applicable character differences can be used to distinguish the two clades. Despite confusing similarities in the worker caste Colobopsis and Camponotus retain diagnostic differences in their larvae and pupae.
C1 [Ward, Philip S.] Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA.
[Blaimer, Bonnie B.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Fisher, Brian L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA.
RP Ward, PS (reprint author), Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA.
EM psward@ucdavis.edu; bonnieblaimer@gmail.com; bfisher@calacademy.org
FU NSF [EF-0431330, DEB-0842204, DEB-1354996]
FX For contributing ant specimens for morphological and molecular work we
are grateful to Alan Andersen, Rumsais Blatrix, Marek Borowiec, Chris
Burwell, Alfred Buschinger, Dinah Davidson, Stephane DeGreef, Flavia
Esteves, Linda Farley, Dave General, Peter Hawkes, Ulrich Maschwitz,
Dave Olson, Christian Peeters, Mike Sharkey, Alberto Tinaut, Simon van
Noort, and Alex Wild. We thank Barry Bolton, Brendon Boudinot, Jack
Longino, and an anonymous reviewer for comments on the manuscript. This
work was supported in part by NSF grants EF-0431330 (to Sean Brady, Ted
Schultz, BLF and PSW), DEB-0842204 (to BLF and PSW), and DEB-1354996 (to
Jack Longino and PSW).
NR 45
TC 9
Z9 9
U1 5
U2 13
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 2
PY 2016
VL 4072
IS 3
BP 343
EP 357
PG 15
WC Zoology
SC Zoology
GA DC7HP
UT WOS:000369390800004
PM 27395929
ER
PT J
AU Rebollar, EA
Antwis, RE
Becker, MH
Belden, LK
Bletz, MC
Brucker, RM
Harrison, XA
Hughey, MC
Kueneman, JG
Loudon, AH
McKenzie, V
Medina, D
Minbiole, KPC
Rollins-Smith, LA
Walke, JB
Weiss, S
Woodhams, DC
Harris, RN
AF Rebollar, Eria A.
Antwis, Rachael E.
Becker, Matthew H.
Belden, Lisa K.
Bletz, Molly C.
Brucker, Robert M.
Harrison, Xavier A.
Hughey, Myra C.
Kueneman, Jordan G.
Loudon, Andrew H.
McKenzie, Valerie
Medina, Daniel
Minbiole, Kevin P. C.
Rollins-Smith, Louise A.
Walke, Jenifer B.
Weiss, Sophie
Woodhams, Douglas C.
Harris, Ried N.
TI Using "Omics" and Integrated Multi-Omics Approaches to Guide Probiotic
Selection to Mitigate Chytridiomycosis and Other Emerging Infectious
Diseases
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Review
DE probiotics; emerging diseases; metagenomics; transcriptomics;
metabolomics; amphibians
ID PATHOGEN BATRACHOCHYTRIUM-DENDROBATIDIS; SALAMANDERS PLETHODON-CINEREUS;
SKIN BACTERIAL COMMUNITIES; LOCAL SIMILARITY ANALYSIS; INNATE IMMUNE
DEFENSES; HUMAN GUT MICROBIOME; FROG-KILLING FUNGUS; SYMBIOTIC BACTERIA;
AMPHIBIAN CHYTRIDIOMYCOSIS; ANTIMICROBIAL PEPTIDE
AB Emerging infectious diseases in wildlife are responsible for massive population declines. In amphibians, chytridiomycosis caused by Batrachochytrium dendrobatidis, Bd, has severely affected many amphibian populations and species around the world. One promising management strategy is probiotic bioaugmentation of antifungal bacteria on amphibian skin. In vivo experimental trials using bioaugmentation strategies have had mixed results, and therefore a more informed strategy is needed to select successful probiotic candidates. Metagenomic, transcriptomic, and metabolomic methods, colloquially called "omics," are approaches that can better inform probiotic selection and optimize selection protocols. The integration of multiple omic data using bioinformatic and statistical tools and in silico models that link bacterial community structure with bacterial defensive function can allow the identification of species involved in pathogen inhibition. We recommend using 16S rRNA gene amplicon sequencing and methods such as indicator species analysis, the Kolmogorov-Smirnov Measure, and co-occurrence networks to identify bacteria that are associated with pathogen resistance in field surveys and experimental trials. In addition to 16S amplicon sequencing, we recommend approaches that give insight into symbiont function such as shotgun metagenomics, metatranscriptomics, or metabolomics to maximize the probability of finding effective probiotic candidates, which can then be isolated in culture and tested in persistence and clinical trials. An effective mitigation strategy to ameliorate chytridiomycosis and other emerging infectious diseases is necessary; the advancement of omic methods and the integration of multiple omic data provide a promising avenue toward conservation of imperiled species.
C1 [Rebollar, Eria A.; Harris, Ried N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA.
[Antwis, Rachael E.] North West Univ, Unit Environm Sci & Management, Potchefstroom, South Africa.
[Antwis, Rachael E.; Harrison, Xavier A.] Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England.
[Antwis, Rachael E.] Univ Salford, Sch Environm & Life Sci, Salford M5 4WT, Lancs, England.
[Becker, Matthew H.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
[Belden, Lisa K.; Hughey, Myra C.; Medina, Daniel; Walke, Jenifer B.] Virginia Tech, Dept Biol Sci, Blacksburg, VA USA.
[Bletz, Molly C.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, Pockelsstr 10A, Braunschweig, Germany.
[Brucker, Robert M.] Harvard Univ, Rowland Inst, Cambridge, MA 02138 USA.
[Kueneman, Jordan G.; McKenzie, Valerie] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Loudon, Andrew H.] Univ British Columbia, Dept Zool, Biodivers Res Ctr, Vancouver, BC, Canada.
[Minbiole, Kevin P. C.] Villanova Univ, Dept Chem, Villanova, PA 19085 USA.
[Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Pathol Microbiol & Immunol, 221 Kirkland Hall, Nashville, TN 37235 USA.
[Rollins-Smith, Louise A.] Vanderbilt Univ, Sch Med, Dept Biol Sci, Dept Pediat, Nashville, TN 37212 USA.
[Weiss, Sophie] Univ Colorado, Dept Chem & Biol Engn, Boulder, CO 80309 USA.
[Woodhams, Douglas C.] Univ Massachusetts, Dept Biol, Boston, MA 02125 USA.
RP Rebollar, EA (reprint author), James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA.
EM ea.rebollar@gmail.com
FU NSF Dimensions in Biodiversity Program [DEB-1136602, DEB-1136640,
DEB-1136662]; German Academic Exchange Service (DAAD); German Research
Foundation (DIG); NSF [IOS-1121758]
FX This project was funded by the NSF Dimensions in Biodiversity Program:
DEB-1136602 to RH, DEB-1136640 to LB and DEB-1136662 to KM. MCB is
supported by the German Academic Exchange Service (DAAD) and The German
Research Foundation (DIG). LR-S is supported by NSF grant IOS-1121758.
NR 201
TC 7
Z9 7
U1 18
U2 91
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1664-302X
J9 FRONT MICROBIOL
JI Front. Microbiol.
PD FEB 2
PY 2016
VL 7
AR 68
DI 10.3389/fmicb.2016.00063
PG 19
WC Microbiology
SC Microbiology
GA DC3IO
UT WOS:000369113200003
PM 26870025
ER
PT J
AU Liu, HB
Takami, M
Kudo, T
Hashimoto, J
Dong, RB
Vorobyov, EI
Pyo, TS
Fukagawa, M
Tamura, M
Henning, T
Dunham, MM
Karr, JL
Kusakabe, N
Tsuribe, T
AF Liu, Hauyu Baobab
Takami, Michihiro
Kudo, Tomoyuki
Hashimoto, Jun
Dong, Ruobing
Vorobyov, Eduard I.
Pyo, Tae-Soo
Fukagawa, Misato
Tamura, Motohide
Henning, Thomas
Dunham, Michael M.
Karr, Jennifer L.
Kusakabe, Nobuhiko
Tsuribe, Toru
TI Circumstellar disks of the most vigorously accreting young stars
SO SCIENCE ADVANCES
LA English
DT Article
ID FU ORIONIS STARS; AURIGA MOLECULAR CLOUD; LOW-MASS STARS; PLANET
FORMATION; EVOLUTION; OUTBURSTS; MODELS; ORI; FRAGMENTATION; CONSTRAINTS
AB Stars may not accumulate their mass steadily, as was previously thought, but in a series of violent events manifesting themselves as sharp stellar brightening. These events can be caused by fragmentation due to gravitational instabilities in massive gaseous disks surrounding young stars, followed by migration of dense gaseous clumps onto the star. Our high-resolution near-infrared imaging has verified the presence of the key associated features, large-scale arms and arcs surrounding four young stellar objects undergoing luminous outbursts. Our hydrodynamics simulations and radiative transfer models show that these observed structures can indeed be explained by strong gravitational instabilities occurring at the beginning of the disk formation phase. The effect of those tempestuous episodes of disk evolution on star and planet formation remains to be understood.
C1 [Liu, Hauyu Baobab; Takami, Michihiro; Dong, Ruobing; Karr, Jennifer L.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Kudo, Tomoyuki; Hashimoto, Jun; Pyo, Tae-Soo; Fukagawa, Misato; Tamura, Motohide; Kusakabe, Nobuhiko] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Dong, Ruobing] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Vorobyov, Eduard I.] Univ Vienna, Dept Astrophys, A-1010 Vienna, Austria.
[Vorobyov, Eduard I.] Southern Fed Univ, Phys Res Inst, Rostov Na Donu 344006, Russia.
[Tamura, Motohide] Univ Tokyo, Tokyo 1138654, Japan.
[Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tsuribe, Toru] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3100056, Japan.
RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
EM baobabyoo@gmail.com
NR 66
TC 7
Z9 7
U1 0
U2 0
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 2375-2548
J9 SCI ADV
JI Sci. Adv.
PD FEB
PY 2016
VL 2
IS 2
AR e1500875
DI 10.1126/sciadv.1500875
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DP7YU
UT WOS:000378715900008
PM 26989772
ER
PT J
AU Martinsen, ES
McInerney, N
Brightman, H
Ferebee, K
Walsh, T
McShea, WJ
Forrester, TD
Ware, L
Joyner, PH
Perkins, SL
Latch, EK
Yabsley, MJ
Schall, JJ
Fleischer, RC
AF Martinsen, Ellen S.
McInerney, Nancy
Brightman, Heidi
Ferebee, Ken
Walsh, Tim
McShea, William J.
Forrester, Tavis D.
Ware, Lisa
Joyner, Priscilla H.
Perkins, Susan L.
Latch, Emily K.
Yabsley, Michael J.
Schall, Joseph J.
Fleischer, Robert C.
TI Hidden in plain sight: Cryptic and endemic malaria parasites in North
American white-tailed deer (Odocoileus virginianus)
SO SCIENCE ADVANCES
LA English
DT Article
ID SOUTHEASTERN UNITED-STATES; HISTORICAL BIOGEOGRAPHY; PLASMODIUM;
MITOCHONDRIAL; IDENTIFICATION; INFECTIONS; SPECIATION; PHYLOGENY;
NUCLEAR; ORIGIN
AB Malaria parasites of the genus Plasmodium are diverse in mammal hosts, infecting five mammalian orders in the Old World, but were long considered absent from the diverse deer family (Cervidae) and from New World mammals. There was a description of a Plasmodium parasite infecting a single splenectomized white-tailed deer (WTD; Odocoileus virginianus) in 1967 but none have been reported since, which has proven a challenge to our understanding of malaria parasite biogeography. Using both microscopy and polymerase chain reaction, we screened a large sample of native and captive ungulate species from across the United States for malaria parasites. We found a surprisingly high prevalence (up to 25%) and extremely low parasitemia of Plasmodium parasites in WTD throughout the eastern United States. We did not detect infections in the other ungulate species nor in western WTD. We also isolated the parasites from the mosquito Anopheles punctipennis. Morphologically, the parasites resemble the parasite described in 1967, Plasmodium odocoilei. Our analysis of the cytochrome b gene revealed two divergent Plasmodium clades in WTD representative of species that likely diverged 2.3 to 6 million years ago, concurrent with the arrival of the WTD ancestor into North America across Beringia. Multigene phylogenetic analysis placed these clades within the larger malaria parasite clade. We document Plasmodium parasites to be common in WTD, endemic to the New World, and as the only known malaria parasites from deer (Cervidae). These findings reshape our knowledge of the phylogeography of the malaria parasites and suggest that other mammal taxa may harbor infection by endemic and occult malaria parasites.
C1 [Martinsen, Ellen S.; McInerney, Nancy; Brightman, Heidi; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
[Ferebee, Ken] Rock Creek Natl Pk, 3545 Williamsburg Lane, Washington, DC 20008 USA.
[Walsh, Tim] Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20560 USA.
[McShea, William J.; Forrester, Tavis D.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Conservat Ecol Ctr, Front Royal, VA 22630 USA.
[Ware, Lisa; Joyner, Priscilla H.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Dept Conservat Med, Front Royal, VA 22630 USA.
[Perkins, Susan L.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, Cent Pk West & 79th St, New York, NY 10024 USA.
[Latch, Emily K.] Univ Wisconsin, Dept Biol Sci, Behav & Mol Ecol Res Grp, 3209 North Maryland Ave, Milwaukee, WI 53211 USA.
[Yabsley, Michael J.] Univ Georgia, Coll Vet Med, Dept Populat Hlth, Southeastern Cooperat Wildlife Dis Study, Athens, GA 30602 USA.
[Yabsley, Michael J.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA.
[Schall, Joseph J.] Univ Vermont, Dept Biol, Marsh Life Sci Bldg, Burlington, VT 05405 USA.
[Brightman, Heidi] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
RP Martinsen, ES (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
EM martinsene@si.edu
NR 34
TC 2
Z9 2
U1 3
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 2375-2548
J9 SCI ADV
JI Sci. Adv.
PD FEB
PY 2016
VL 2
IS 2
AR e1501486
DI 10.1126/sciadv.1501486
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DP7YU
UT WOS:000378715900034
PM 26989785
ER
PT J
AU Hirashita, H
Koch, PM
Matsushita, S
Takakuwa, S
Nakamura, M
Asada, K
Liu, HB
Urata, Y
Wang, MJ
Wang, WH
Takahashi, S
Tang, YW
Chang, HH
Huang, K
Morata, O
Otsuka, M
Lin, KY
Tsai, AL
Lin, YT
Srinivasan, S
Martin-Cocher, P
Pu, HY
Kemper, F
Patel, N
Grimes, P
Huang, YD
Han, CC
Huang, YR
Nishioka, H
Lin, LCC
Zhang, QZ
Keto, E
Burgos, R
Chen, MT
Inoue, M
Ho, PTP
AF Hirashita, Hiroyuki
Koch, Patrick M.
Matsushita, Satoki
Takakuwa, Shigehisa
Nakamura, Masanori
Asada, Keiichi
Liu, Hauyu Baobab
Urata, Yuji
Wang, Ming-Jye
Wang, Wei-Hao
Takahashi, Satoko
Tang, Ya-Wen
Chang, Hsian-Hong
Huang, Kuiyun
Morata, Oscar
Otsuka, Masaaki
Lin, Kai-Yang
Tsai, An-Li
Lin, Yen-Ting
Srinivasan, Sundar
Martin-Cocher, Pierre
Pu, Hung-Yi
Kemper, Francisca
Patel, Nimesh
Grimes, Paul
Huang, Yau-De
Han, Chih-Chiang
Huang, Yen-Ru
Nishioka, Hiroaki
Lin, Lupin Chun-Che
Zhang, Qizhou
Keto, Eric
Burgos, Roberto
Chen, Ming-Tang
Inoue, Makoto
Ho, Paul T. P.
TI First-generation science cases for ground-based terahertz telescopes
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Review
DE dust, extinction; galaxies: ISM-ISM: lines and bands; submillimeter:
general; telescopes
ID GAMMA-RAY BURST; SPECTRAL ENERGY-DISTRIBUTIONS; HUBBLE-SPACE-TELESCOPE;
COMPACT DWARF GALAXIES; STAR-FORMING REGIONS; GOULD BELT SURVEY; ACTIVE
GALACTIC NUCLEI; DARK CLOUD CORES; 850 MU-M; DIFFUSE INTERSTELLAR-MEDIUM
AB Ground-based observations at terahertz (THz) frequencies are a newly explorable area of astronomy in the coming decades. We discuss science cases for a first-generation 10-m class THz telescope, focusing on the Greenland Telescope as an example of such a facility. We propose science cases and provide quantitative estimates for each case. The largest advantage of ground-based THz telescopes is their higher angular resolution (similar to 4 '' for a 10-m dish), as compared to space or airborne THz telescopes. Thus, high-resolution mapping is an important scientific argument. In particular, we can isolate zones of interest for Galactic and extragalactic star-forming regions. The THz windows are suitable for observations of high-excitation CO lines and [NII] 205-mu m lines, which are scientifically relevant tracers of star formation and stellar feedback. Those lines are the brightest lines in the THz windows, so they are suitable for the initiation of ground-based THz observations. THz polarization of star-forming regions can also be explored since it traces the dust population contributing to the THz spectral peak. For survey-type observations, we focus on "sub-THz" extragalactic surveys, the uniqueness of which is detecting galaxies at redshifts z similar to 1-2, where the dust emission per comoving volume is the largest in the history of the Universe. Finally we explore possibilities of flexible time scheduling, which enables us to monitor active galactic nuclei, and to target gamma-ray burst afterglows. For these objects, THz and submillimeter wavelength ranges have not yet been explored.
C1 [Hirashita, Hiroyuki; Koch, Patrick M.; Matsushita, Satoki; Takakuwa, Shigehisa; Nakamura, Masanori; Asada, Keiichi; Liu, Hauyu Baobab; Urata, Yuji; Wang, Ming-Jye; Wang, Wei-Hao; Tang, Ya-Wen; Chang, Hsian-Hong; Morata, Oscar; Otsuka, Masaaki; Lin, Kai-Yang; Lin, Yen-Ting; Srinivasan, Sundar; Martin-Cocher, Pierre; Pu, Hung-Yi; Kemper, Francisca; Huang, Yau-De; Han, Chih-Chiang; Huang, Yen-Ru; Nishioka, Hiroaki; Lin, Lupin Chun-Che; Chen, Ming-Tang; Inoue, Makoto; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Urata, Yuji; Tsai, An-Li] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
[Takahashi, Satoko] Joint ALMA Observ, Alonso de Cordova 3108, Santiago, Chile.
[Takahashi, Satoko] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Huang, Kuiyun] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei 24449, Taiwan.
[Patel, Nimesh; Grimes, Paul; Zhang, Qizhou; Keto, Eric; Burgos, Roberto] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Ho, Paul T. P.] East Asian Observ, 660 N Aohoku Pl, Hilo, HI 96720 USA.
RP Hirashita, H (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM hirashita@asiaa.sinica.edu.tw
RI Kemper, Francisca/D-8688-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Zhang, Qizhou/0000-0003-2384-6589
FU Ministry of Science and Technology (MoST) in Taiwan
[102-2119-M-001-006-MY3, 103-2112-M-001-032-MY3,
102-2119-M-001-007-MY3]; grant MoST [103-2119-M-001-009]; Academia
Sinica Career Development Award
FX We are grateful to the anonymous referee for useful comments and R.
Blundell and S. Paine for continuous support. We thank the Ministry of
Science and Technology (MoST) in Taiwan for support through grants
102-2119-M-001-006-MY3 (HH), 103-2112-M-001-032-MY3 (SM) and
102-2119-M-001-007-MY3 (WHW). PMK acknowledges support from grant MoST
103-2119-M-001-009 and an Academia Sinica Career Development Award.
NR 284
TC 1
Z9 1
U1 2
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB
PY 2016
VL 68
IS 1
AR R1
DI 10.1093/pasj/psv115
PG 41
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ9ZE
UT WOS:000374571300003
ER
PT J
AU Ichikawa, K
Ueda, J
Shidatsu, M
Kawamuro, T
Matsuoka, K
AF Ichikawa, Kohei
Ueda, Junko
Shidatsu, Megumi
Kawamuro, Taiki
Matsuoka, Kenta
TI Signs of active galactic nucleus quenching in a merger remnant with
radio jets
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies: active; galaxies: nuclei; infrared: galaxies
ID SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; X-RAY CORRELATION; HOST
GALAXIES; INFRARED GALAXIES; MU-M; SPECTRAL CLASSIFICATION; FUNDAMENTAL
PLANE; EMISSION; ACCRETION
AB We investigate optical, infrared, and radio active galactic nucleus (AGN) signs in the merger remnant Arp 187, which hosts luminous jets launched in the order of 10(5) yr ago but whose present-day AGN activity is still unknown. We find AGN signs from the optical Baldwin-Phillips-Telervich diagram and infrared [O IV] 25.89 mu m line, originating from the narrow line regions of AGN. On the other hand, Spitzer/IRS show host galaxy dominated spectra, suggesting that the thermal emission from the AGN torus is considerably small or already diminished. Combining the black holemass, the upper limit of radio luminosity of the core, and the fundamental plane of the black hole enables us to estimate X-ray luminosity, which gives < 10(40) erg s(-1). Those results suggest that the AGN activity of Arp 187 has already been quenched, but the narrow line region is still alive owing to the time delay of emission from the past AGN activity.
C1 [Ichikawa, Kohei; Ueda, Junko] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Ueda, Junko] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Shidatsu, Megumi] RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
[Kawamuro, Taiki; Matsuoka, Kenta] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
RP Ichikawa, K (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM kohei.ichikawa@nao.ac.jp
RI Shidatsu, Megumi/C-5742-2017
FU National Aeronautics and Space Administration; [40756293]
FX We are grateful for useful comments from the anonymous referee. We thank
Yoshiki Matsuoka, Tohru Nagao, Ryou Ohsawa, Kouji Ohta, Chris Packham,
and Yoshihiro Ueda for valuable comments and discussions. This research
has made use of the NASA/IPAC Extragalactic Database (NED) which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. This work was partly supported by Grant-in-Aid for
Scientific Research 40756293 (K.I.).
NR 63
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB
PY 2016
VL 68
IS 1
AR 9
DI 10.1093/pasj/psv112
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ9ZE
UT WOS:000374571300012
ER
PT J
AU Fuxjager, MJ
Lee, JH
Chan, TM
Bahn, JH
Chew, JG
Xiao, XS
Schlinger, BA
AF Fuxjager, Matthew J.
Lee, Jae-Hyung
Chan, Tak-Ming
Bahn, Jae Hoon
Chew, Jenifer G.
Xiao, Xinshu
Schlinger, Barney A.
TI Research Resource: Hormones, Genes, and Athleticism: Effect of Androgens
on the Avian Muscular Transcriptome
SO MOLECULAR ENDOCRINOLOGY
LA English
DT Article
ID GOLDEN-COLLARED MANAKINS; ELABORATE MALE COURTSHIP; SPEED VIDEO
ANALYSIS; SKELETAL-MUSCLE; MANACUS-VITELLINUS; LIPID-METABOLISM; ZEBRA
FINCH; DIFFERENTIAL EXPRESSION; FEMALE CHOICE; TESTOSTERONE
AB Male vertebrate social displays vary from physically simple to complex, with the latter involving exquisite motor command of the body and appendages. Studies of these displays have, in turn, provided substantial insight into neuromotor mechanisms. The neotropical golden-collared manakin (Manacus vitellinus) has been used previously as a model to investigate intricate motor skills because adult males of this species perform an acrobatic and androgen-dependent courtship display. To support this behavior, these birds express elevated levels of androgen receptors (AR) in their skeletal muscles. Here we use RNA sequencing to explore how testosterone (T) modulates the muscular transcriptome to support male manakin courtship displays. In addition, we explore how androgens influence gene expression in the muscles of the zebra finch (Taenopygia guttata), a model passerine bird with a limited courtship display and minimal muscle AR. We identify androgen-dependent, muscle-specific gene regulation in both species. In addition, we identify manakin-specific effects that are linked to muscle use during the manakin display, including androgenic regulation of genes associated with muscle fiber contractility, cellular homeostasis, and energetic efficiency. Overall, our results point to numerous genes and gene networks impacted by androgens in male birds, including some that underlie optimal muscle function necessary for performing acrobatic display routines. Manakins are excellent models to explore gene regulation promoting athletic ability.
C1 [Fuxjager, Matthew J.] Wake Forest Univ, Dept Biol, Box 7325 Reynolda Stn, Winston Salem, NC 27109 USA.
[Lee, Jae-Hyung] Kyung Hee Univ, Dept Life & Nanopharmaceut Sci, Sch Dent, Seoul 130701, South Korea.
[Lee, Jae-Hyung] Kyung Hee Univ, Dept Maxillofacial Biomed Engn, Sch Dent, Seoul 130701, South Korea.
[Fuxjager, Matthew J.; Lee, Jae-Hyung; Chan, Tak-Ming; Bahn, Jae Hoon; Chew, Jenifer G.; Xiao, Xinshu; Schlinger, Barney A.] Univ Calif Los Angeles, Brain Res Inst, Dept Integrat Biol & Physiol, Los Angeles, CA 90095 USA.
[Fuxjager, Matthew J.; Schlinger, Barney A.] Univ Calif Los Angeles, Neuroendocrinol Lab, Brain Res Inst, Los Angeles, CA 90095 USA.
[Schlinger, Barney A.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Fuxjager, MJ (reprint author), Wake Forest Univ, Dept Biol, Box 7325 Reynolda Stn, Winston Salem, NC 27109 USA.; Xiao, XS; Schlinger, BA (reprint author), Univ Calif Los Angeles, Brain Res Inst, Dept Integrat Biol & Physiol, Los Angeles, CA 90095 USA.; Schlinger, BA (reprint author), Univ Calif Los Angeles, Neuroendocrinol Lab, Brain Res Inst, Los Angeles, CA 90095 USA.; Schlinger, BA (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
EM mfoxhunter@gmail.com; gxxiao@ucla.edu; schlinge@lifesci.ucla.edu
OI Lee, Jae-Hyung/0000-0002-5085-6988
FU National Institutes of Health [T32 HD007228, R01HG006264]; Wake Forest
University; National Science Foundation [IOS-0646459, 1262134]; Ministry
of Health and Welfare [HI14C0175]
FX This work was supported by National Institutes of Health Training Grant
T32 HD007228 awarded to the Laboratory of Neuroendocrinology at the
University of California, Los Angeles, and Wake Forest University
institutional start-up funds supported M.J.F. This work was also
supported by National Science Foundation Grants IOS-0646459 (to B.A.S.)
and 1262134 (to X.X.) and National Institutes of Health Grant
R01HG006264 (to X.X.). Ministry of Health and Welfare Grant HI14C0175
(Republic of Korea) (to J.-H.L.) also supported the research.
NR 82
TC 3
Z9 3
U1 2
U2 4
PU ENDOCRINE SOC
PI WASHINGTON
PA 2055 L ST NW, SUITE 600, WASHINGTON, DC 20036 USA
SN 0888-8809
J9 MOL ENDOCRINOL
JI Mol. Endocrinol.
PD FEB
PY 2016
VL 30
IS 2
BP 254
EP 271
DI 10.1210/me.2015-1270
PG 18
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA DN6SN
UT WOS:000377206500009
PM 26745669
ER
PT J
AU Arias, CF
Van Belleghem, S
McMillan, WO
AF Arias, Carlos F.
Van Belleghem, Steven
McMillan, W. Owen
TI Genomics at the evolving species boundary
SO CURRENT OPINION IN INSECT SCIENCE
LA English
DT Article
ID WITH-GENE-FLOW; REPRODUCTIVE ISOLATION; HYBRID ZONES; HELICONIUS
BUTTERFLIES; DROSOPHILA-PSEUDOOBSCURA; SPECIATION CONTINUUM; POPULATION
GENOMICS; NATURAL-SELECTION; PATTERN MIMICRY; CLIMATE-CHANGE
AB Molecular studies on hybridization date back to Dobzhansky who compared chromosomal banding patterns to determine if interspecific gene flow occurred in nature [1]. Now, the advent of high-throughput sequencing provides increasingly fine insights into genomic differentiation between incipient taxa that are changing our view of adaptation and speciation and the links between the two. Empirical data from hybridizing taxa demonstrate highly heterogeneous patterns of genomic differentiation. Although underlining reasons for this heterogeneity are complex, studies of hybridizing taxa offers some of the best insights into the regions of the genome under divergent selection and the role these regions play in species boundaries. The challenge moving forward is to develop a better theoretical framework that fully leverages these powerful natural experiments.
C1 [Arias, Carlos F.; Van Belleghem, Steven; McMillan, W. Owen] Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
[Van Belleghem, Steven] Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England.
[Van Belleghem, Steven] Univ Puerto Rico, Dept Biol, Ctr Appl Trop Ecol & Conservat, Rio Piedras, PR USA.
[Arias, Carlos F.] Univ Rosario, Fac Nat Sci & Math, Biol Program, Carrera 24 63c-69, Bogota 111221, Colombia.
RP McMillan, WO (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM mcmillano@si.edu
OI Arias, Carlos Francisco/0000-0001-5925-0985
FU United States National Science Foundation [DEB 1257689]; Smithsonian
Tropical Research Institute; Smithsonian Institution's Competitive
Grants program
FX This work was supported by funding from the United States National
Science Foundation (DEB 1257689), the Smithsonian Tropical Research
Institute, and the Smithsonian Institution's Competitive Grants program.
NR 76
TC 2
Z9 2
U1 8
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2214-5745
EI 2214-5753
J9 CURR OPIN INSECT SCI
JI Curr. Opin. Insect Sci.
PD FEB
PY 2016
VL 13
BP 7
EP 15
DI 10.1016/j.cois.2015.10.004
PG 9
WC Biology; Ecology; Entomology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Entomology
GA DM4FL
UT WOS:000376301800004
PM 27436548
ER
PT J
AU Kohri, K
Ioka, K
Fujita, Y
Yamazaki, R
AF Kohri, Kazunori
Ioka, Kunihito
Fujita, Yutaka
Yamazaki, Ryo
TI Can we explain AMS-02 antiproton and positron excesses simultaneously by
nearby supernovae without pulsars or dark matter?
SO PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS
LA English
DT Article
ID COSMIC-RAY POSITRONS; YOUNG STARS; ELECTRONS; SPECTRUM; ORIGIN;
ENERGIES; REMNANTS
AB We explain the excess of the antiproton fraction recently reported by the AMS-02 experiment by considering collisions between cosmic-ray protons accelerated by a local supernova remnant and the surrounding dense cloud. The same "pp collisions" provide the right ratio of daughter particles to fit the observed positron excess simultaneously in the natural model parameters. The supernova happened in relatively lower metallicity than the major cosmic-ray sources. The cutoff energy of electrons marks the supernova age of similar to 10(5) years, while the antiproton excess may extend to higher energy. Both antiproton and positron fluxes are completely consistent with our predictions in an earlier paper [Y. Fujita et al., Phys. Rev. D 80, 063003 (2009) [arXiv:0903.5298 [astro-ph.HE]]].
C1 [Kohri, Kazunori; Ioka, Kunihito] KEK, IPNS, Ctr Theory, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan.
[Kohri, Kazunori; Ioka, Kunihito] Sokendai, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan.
[Fujita, Yutaka] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Yamazaki, Ryo] Aoyama Gakuin Univ, Dept Math & Phys, Yokohama, Kanagawa 2525258, Japan.
[Yamazaki, Ryo] Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA.
RP Kohri, K (reprint author), KEK, IPNS, Ctr Theory, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan.; Kohri, K (reprint author), Sokendai, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan.
EM kohri@post.kek.jp
NR 53
TC 8
Z9 8
U1 0
U2 3
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 2050-3911
J9 PROG THEOR EXP PHYS
JI Prog. Theor. Exp. Phys.
PD FEB
PY 2016
IS 2
AR 021E01
DI 10.1093/ptep/ptv193
PG 8
WC Physics, Multidisciplinary; Physics, Particles & Fields
SC Physics
GA DH2JW
UT WOS:000372612400007
ER
PT J
AU Nagashima, JB
Hansen, BS
Songsasen, N
Travis, AJ
Place, NJ
AF Nagashima, J. B.
Hansen, B. S.
Songsasen, N.
Travis, A. J.
Place, N. J.
TI Anti-Mullerian Hormone in the Domestic Dog during the Anestrus to
Oestrous Transition
SO REPRODUCTION IN DOMESTIC ANIMALS
LA English
DT Article
ID IN-VITRO FERTILIZATION; INHIBITING SUBSTANCE; LUTEINIZING-HORMONE;
MENSTRUAL-CYCLE; CANINE OOCYTES; FOLLICLE RECRUITMENT; NUCLEAR
MATURATION; SIBERIAN HAMSTERS; ENDOCRINE MARKER; EMBRYO QUALITY
AB The reproductive cycle of the domestic dog features a long period of relative ovarian inactivity or anestrus. The mechanism of anestrous termination/oestrous resumption is not yet fully understood, which presents a challenge to the development of oestrous induction protocols. In this study, we assess the possibility that anti-Mullerian hormone (AMH) might play a role in this transition by characterizing its patterns of expression in the circulation during the transition from anestrus to oestrous and in all stages of ovarian follicular growth. Serum samples from five beagles (2.0-4.5 years) were collected three times per week at least 30 days prior to the onset of oestrous and assessed for AMH concentrations. Serum AMH concentration increased significantly during the transition from anestrus to proestrus and then declined back to the anestrous baseline beginning on day -4 before the luteinizing hormone surge, which was determined by changes in serum progesterone concentrations. Cortical sections of ovaries from females undergoing routine ovariohysterectomy (aged 8 months-5 years, n = 4) were evaluated for AMH by immunohistochemistry. Pre-antral and small antral follicles were most strongly immunoreactive for AMH. These data suggest that the increase in the number of antral follicles is associated with the rise in serum AMH as the anestrous period comes to an end. The rise in AMH might be useful in predicting the onset of oestrus and therefore assist with the optimization of oestrous induction protocols and possibly other assisted reproductive technologies.
C1 [Nagashima, J. B.; Travis, A. J.] Cornell Univ, James A Baker Inst Anim Hlth, Ithaca, NY 14853 USA.
[Hansen, B. S.; Place, N. J.] Cornell Univ, Dept Populat Med & Diagnost Sci, Ithaca, NY 14853 USA.
[Songsasen, N.] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
[Travis, A. J.] Cornell Univ, Atkinson Ctr Sustainable Future, Ithaca, NY 14853 USA.
RP Place, NJ (reprint author), Cornell Univ, Dept Populat Med & Diagnost Sci, Ithaca, NY 14853 USA.
EM njp27@cornell.edu
FU Cornell University's Diagnostic Endocrinology Laboratory; NIH
[DP-OD-006431]; Cornell University's Baker Institute for Animal Health;
Atkinson Center for a Sustainable Future; Smithsonian Institution
Predoctoral Fellowship
FX This research was supported by Cornell University's Diagnostic
Endocrinology Laboratory (NJP), NIH DP-OD-006431 (AJT), Cornell
University's Baker Institute for Animal Health (AJT), the Atkinson
Center for a Sustainable Future (AJT) and a Smithsonian Institution
Predoctoral Fellowship (JBN).
NR 54
TC 1
Z9 1
U1 1
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0936-6768
EI 1439-0531
J9 REPROD DOMEST ANIM
JI Reprod. Domest. Anim.
PD FEB
PY 2016
VL 51
IS 1
BP 158
EP 164
DI 10.1111/rda.12660
PG 7
WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary
Sciences
SC Agriculture; Reproductive Biology; Veterinary Sciences
GA DH9HR
UT WOS:000373107600022
PM 26708613
ER
PT J
AU Bell, JA
AF Bell, Joshua A.
TI Dystopian realities and archival dreams in the Purari Delta of Papua New
Guinea
SO SOCIAL ANTHROPOLOGY
LA English
DT Article
DE archives; history; ruination; documents; Papua New Guinea
ID EXTRACTION
AB Years of resource extraction by multinational corporations have transformed the Purari Delta into a resource frontier where communities' desires, subjectivities and histories are being unevenly reconfigured. Focusing on the struggles of I'ai communities for recognition by the Papua New Guinean government as traditional resource owners, I examine how, in the wake of the destruction of regional archives and the perceived inaccessibility of PNG's National Archives, men are marshalling new assemblages of evidence: written ancestral histories, heirloom objects, found images and maps. I explore how I'ai men are strategically deploying these materials to actualise their utopian dreams of recognition.
C1 [Bell, Joshua A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC 112, Washington, DC 20560 USA.
RP Bell, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC 112, Washington, DC 20560 USA.
EM bellja@si.edu
NR 54
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0964-0282
EI 1469-8676
J9 SOC ANTHROPOL
JI Soc. Anthropol.
PD FEB
PY 2016
VL 24
IS 1
SI SI
BP 20
EP 35
DI 10.1111/1469-8676.12285
PG 16
WC Anthropology
SC Anthropology
GA DH5ER
UT WOS:000372808800003
ER
PT J
AU Chen, XG
Namjoo, MH
Wang, Y
AF Chen, Xingang
Namjoo, Mohammad Hossein
Wang, Yi
TI Quantum primordial standard clocks
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE inflation; alternatives to inflation; non-gaussianity; cosmological
perturbation theory
ID INFLATIONARY UNIVERSE; GRAVITY-WAVES; PERTURBATIONS; POLARIZATION;
FLATNESS; PARADIGM; HORIZON
AB In this paper, we point out and study a generic type of signals existing in the primordial universe models, which can be used to model-independently distinguish the inflation scenario from alternatives. These signals are generated by massive fields that function as standard clocks. The role of massive fields as standard clocks has been realized in previous works. Although the existence of such massive fields is generic, the previous realizations require sharp features to classically excite the oscillations of the massive clock fields. Here, we point out that the quantum fluctuations of massive fields can actually serve the same purpose as the standard clocks. We show that they are also able to directly record the defining property of the scenario type, namely, the scale factor of the primordial universe as a function of time a(t), but through shape-dependent oscillatory features in non-Gaussianities. Since quantum fluctuating massive fields exist in any realistic primordial universe models, these quantum primordial standard clock signals are present in any inflation models, and should exist quite generally in alternative-to-inflation scenarios as well. However, the amplitude of such signals is very model-dependent.
C1 [Chen, Xingang; Namjoo, Mohammad Hossein] Univ Texas Dallas, Dept Phys, Richardson, TX 75083 USA.
[Chen, Xingang; Namjoo, Mohammad Hossein] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Wang, Yi] Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China.
RP Chen, XG; Namjoo, MH (reprint author), Univ Texas Dallas, Dept Phys, Richardson, TX 75083 USA.; Chen, XG; Namjoo, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.; Wang, Y (reprint author), Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China.
EM xingang.chen@cfa.harvard.edu; mohammad.namjoo@cfa.harvard.edu;
phyw@ust.hk
FU NSF [PHY-1417421]; Research Grants Council (RGC) of Hong Kong
[HKUST4/CRF/13G]; National Science Foundation [PHY-1066293]
FX We thank Nima Arkani-Hamed, Daniel Eisenstein, Avi Loeb, and Juan
Maldacena for helpful discussions. XC and MHN are supported in part by
the NSF grant PHY-1417421. YW is supported by Grant HKUST4/CRF/13G
issued by the Research Grants Council (RGC) of Hong Kong. Part of this
work was performed at the Aspen Center for Physics during the workshop
"Primordial Universe", which is supported by National Science Foundation
grant PHY-1066293.
NR 51
TC 4
Z9 4
U1 3
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD FEB
PY 2016
IS 2
AR 013
DI 10.1088/1475-7516/2016/02/013
PG 35
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DH0IM
UT WOS:000372467600014
ER
PT J
AU Bernal, JL
Verde, L
Cuesta, AJ
AF Luis Bernal, Jose
Verde, Licia
Cuesta, Antonio J.
TI Parameter splitting in dark energy: is dark energy the same in the
background and in the cosmic structures?
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE cosmological parameters from LSS; cosmological parameters from CMBR;
dark energy theory
ID BARYON ACOUSTIC-OSCILLATIONS; WEAK-LENSING MEASUREMENTS; COSMOLOGICAL
CONSTRAINTS; GROWTH-RATE; GALAXY CLUSTERS; REDSHIFT SPACE; CONSTANT;
SUPERNOVAE; GEOMETRY; SAMPLES
AB We perform an empirical consistency test of General Relativity/dark energy by disentangling expansion history and growth of structure constraints. We replace each late universe parameter that describes the behavior of dark energy with two meta-parameters: one describing geometrical information in cosmological probes, and the other controlling the growth of structure. If the underlying model (a standard wCDM cosmology with General Relativity) is correct, that is under the null hypothesis, the two meta-parameters coincide. If they do not, it could indicate a failure of the model or systematics in the data. We present a global analysis using state-of-the-art cosmological data sets which points in the direction that cosmic structures prefer a weaker growth than that inferred by background probes. This result could signify inconsistencies of the model, the necessity of extensions to it or the presence of systematic errors in the data. We examine all these possibilities. The fact that the result is mostly driven by a specific sub-set of galaxy clusters abundance data, points to the need of a better understanding of this probe.
C1 [Luis Bernal, Jose; Verde, Licia; Cuesta, Antonio J.] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain.
[Luis Bernal, Jose] Univ Barcelona, Dept Astron & Meteorol, Marti & Franques 1, E-08028 Barcelona, Spain.
[Verde, Licia] ICREA, E-2308010 Barcelona, Spain.
[Verde, Licia] Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
[Verde, Licia] Harvard Univ, Radcliffe Inst Adv Study, 10 Garden St, Cambridge, MA 02138 USA.
[Verde, Licia] Harvard Smithsonian Ctr Astrophys, ITC, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
RP Bernal, JL; Verde, L; Cuesta, AJ (reprint author), Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain.; Bernal, JL (reprint author), Univ Barcelona, Dept Astron & Meteorol, Marti & Franques 1, E-08028 Barcelona, Spain.; Verde, L (reprint author), ICREA, E-2308010 Barcelona, Spain.; Verde, L (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.; Verde, L (reprint author), Harvard Univ, Radcliffe Inst Adv Study, 10 Garden St, Cambridge, MA 02138 USA.; Verde, L (reprint author), Harvard Smithsonian Ctr Astrophys, ITC, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM joseluis.bernal@icc.ub.edu; liciaverde@icc.ub.edu; ajcuesta@icc.ub.edu
OI Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Verde,
Licia/0000-0003-2601-8770
FU Spanish MINECO [BES-2015-071307]; ESF; CEI UAM-CSIC; European Research
Council under the European Community's Seventh Framework Programme
FP7-IDEAS-Phys.LSS [240117]; Royal Society [IE140357]; ESA Member
States; NASA; Alfred P. Sloan Foundation; National Science Foundation;
U.S. Department of Energy Office of Science; Spanish MINECO of ICCUB
(Unidad de Excelencia "Maria de Maeztu") [AYA2014-58747-P,
MDM-2014-0369]
FX We thank Dragan Huterer for valuable comments on an early version of the
draft which help improve the paper. JLB is supported by the Spanish
MINECO under grant BES-2015-071307, co-funded by the ESF. JLB
acknowledges financial support from CEI UAM-CSIC during part of this
work. LV and AJC are supported by the European Research Council under
the European Community's Seventh Framework Programme FP7-IDEAS-Phys.LSS
240117. Funding for this work was partially provided by the Spanish
MINECO under projects AYA2014-58747-P and MDM-2014-0369 of ICCUB (Unidad
de Excelencia "Maria de Maeztu"). LV acknowledges hospitality of
Imperial Center for Inference and Cosmology and support by Royal Society
grant IE140357. AJC acknowledges hospitality of ITC, Harvard-Smithsonian
Center for Astrophysics, Harvard University.; Based on observations
obtained with Planck (http://www.esa.int/Planck), an ESA science mission
with instruments and contributions directly funded by ESA Member States,
NASA, and Canada.; Funding for SDSS-III has been provided by the Alfred
P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, and the U.S. Department of Energy Office of Science.
The SDSS-III web site is http://www.sdss3.org/.
NR 55
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD FEB
PY 2016
IS 2
AR 059
DI 10.1088/1475-7516/2016/02/059
PG 24
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DH0IM
UT WOS:000372467600060
ER
PT J
AU Campbell, BA
Watters, TR
AF Campbell, Bruce A.
Watters, Thomas R.
TI Phase compensation of MARSIS subsurface sounding data and estimation of
ionospheric properties: New insights from SHARAD results
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE MARSIS; SHARAD; ionosphere; Mars
ID MARTIAN IONOSPHERE; RADAR SOUNDINGS; ECHOES
AB Subsurface radar sounding observations by the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) and Shallow Radar (SHARAD) instruments are affected by ionospheric phase distortions that lead to image blurring and delay offsets. Based on experience with SHARAD image correction, we propose that ionospheric blurring in MARSIS radargrams may be compensated with a model of smoothly varying quadratic phase errors along the track. This method yields well-focused radargrams for geologic interpretation and allows analysis of the validity range for models used to derive total electron content (TEC) from phase distortion terms in previous MARSIS studies. The quadratic term appears to be a good proxy for TEC at solar zenith angles >65 degrees for MARSIS Band 4 (5MHz) and >75 degrees for Band 3 (4MHz). Comparison of MARSIS- and SHARAD-derived TEC values from 2007 to 2014 reveals correlations in seasonal behavior and in the characterization of ionospheric activity due to coronal mass ejections. We also present SHARAD and MARSIS evidence for a persistent region of anomalous radar scattering south of Arsia Mons. These echoes have been previously suggested to arise from refraction of the radar signal by electron density variations. There are no strong signatures, however, in the quadratic image compensation term correlated with the anomalous scattering, suggesting either that electron density variations responsible for refracted signal paths occur primarily in regions offset from the spacecraft track or that these density changes have a minimal impact on the integrated phase distortion of the subspacecraft footprint. We suggest observations and analyses to better constrain the mechanism and timing of such echoes.
C1 [Campbell, Bruce A.; Watters, Thomas R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
EM campbellb@si.edu
NR 25
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB
PY 2016
VL 121
IS 2
BP 180
EP 193
DI 10.1002/2015JE004917
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DH1AQ
UT WOS:000372517200005
ER
PT J
AU Carn, SA
Clarisse, L
Prata, AJ
AF Carn, S. A.
Clarisse, L.
Prata, A. J.
TI Multi-decadal satellite measurements of global volcanic degassing
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Review
DE Satellite remote sensing; Volcanic SO2 emissions; Volcanic degassing;
Volcanic eruptions; Volcanic plumes; Volcanic clouds
ID SULFUR-DIOXIDE EMISSIONS; OZONE MONITORING INSTRUMENT; ASIAN MONSOON
TRANSPORT; STRATOSPHERIC AEROSOL LAYER; INFRARED IMAGING CAMERA;
ATMOSPHERIC WATER-VAPOR; SOUFRIERE-HILLS VOLCANO; SBUV/2 SPECTRAL DATA;
EL-CHICHON; MOUNT-PINATUBO
AB Satellite instruments have been providing measurements of global volcanic emissions of sulfur dioxide (SO2) since 1978, based on observations in the ultraviolet (UV), infrared (IR) and microwave spectral bands. We review recent advances in satellite remote sensing of volcanic gases, focusing on increased instrument sensitivity to tropospheric SO2 emissions and techniques to determine volcanic plume altitude. A synthesis of similar to 36 years of global UV, IR and microwave satellite measurements yields an updated assessment of the volcanic SO2 flux to the upper troposphere and lower stratosphere (UTLS) between 1978 and 2014 (similar to 1-2 Tg/yr). The present availability of multiple UV and IR satellite SO2 products provides increased confidence in calculated SO2 loadings for many eruptions. We examine the temporal and latitudinal distribution of volcanic SO2 emissions and reassess the relationship between eruptive SO2 discharge and eruption magnitude, finding a first-order correlation between SO2 emission and volcanic explosivity index (VEI), but with significant scatter. Based on the observed SO2-VEI relation, we estimate the fraction of eruptive SO2 emissions released by the smallest eruptions (similar to 0.48 Tg/yr), which is not recorded by satellite observations. A detailed breakdown of the sources of measured SO2 emissions reveals intuitively expected correlations between eruption frequency, SO2 loading and volcanic degassing style. We discuss new constraints on e-folding times for SO2 removal in volcanic plumes, and highlight recent measurements of volcanic hydrogen chloride (HCI) injections into the UTLS. An analysis of passive volcanic emissions of SO2 detected in Ozone Monitoring Instrument (OMI) SO2 data since 2004 provides new insight into the location and stability of the dominant sources of volcanic SO2 over the past decade. Since volcanic SO2 emissions constitute a random, highly variable perturbation to the atmosphere-climate system, continued monitoring of volcanic SO2 emissions from space by multiple UV and IR instruments to extend the current multi-decadal record is essential, and near-global, geostationary measurements of SO2 may be available by the end of the current decade. (C) 2016 The Authors. Published by Elsevier B.V.
C1 [Carn, S. A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
[Carn, S. A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Clarisse, L.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, Spect Atmosphere, Brussels, Belgium.
[Prata, A. J.] Nicamica Aviat AS, Kjeller, Norway.
RP Carn, SA (reprint author), Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
EM scarn@mtu.edu
FU Belgian Fonds de la Recherche Scientifique (F.R.S-FNRS); [NNX10AG60G];
[NNX11AK95G]; [NNX13AF50G]
FX We acknowledge editors Tim Horscroft and Alessandro Aiuppa for inviting
this review article. NASA has provided generous support of
satellite-based volcanic SO2 measurements to S.A.C, including
recent grants NNX10AG60G (A Combined EOS Data and GEOS-Chem Modeling
Study of the Direct Radiative Forcing of Volcanic Sulfate Aerosois; PI:
J. Wang), NNX11AK95G (Continuation of Long-Term Sulfur Dioxide EDR with
the SNPP/OMPS Nadir Mapper; PI: K. Yang) and NNX13AF50G (Multi-Decadal
Sulfur Dioxide Climatology from Satellite Instruments; PI: N.A.
Krotkov). L.C. is a research associate supported by the Belgian Fonds de
la Recherche Scientifique (F.R.S-FNRS). We thank Jean-Paul Vernier (NASA
Langley) for providing recent stratospheric aerosol data and Mauro
Tomasi (ULB) for collating the data used to produce an earlier version
of Fig. 14. David Pyle and an anonymous reviewer provided thorough and
constructive reviews of the paper. The article was written whilst the
first author was on sabbatical at the Department of Mineral Sciences
(DMS), National Museum of Natural History, Smithsonian Institution, and
SAC acknowledges the Smithsonian for a visiting fellowship and the DMS
staff for their hospitality. The volcanic SO2 emissions
database described in this paper is available from the NASA Goddard
Earth Sciences (GES) Data and Information Services Center (DISK) as a
level 4 MEaSUREs (Making Earth System Data Records for Use in Research
Environments) data product (Cam, 2015c).
NR 289
TC 15
Z9 15
U1 9
U2 22
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD FEB 1
PY 2016
VL 311
BP 99
EP 134
DI 10.1016/j.jvolgeores.2016.01.002
PG 36
WC Geosciences, Multidisciplinary
SC Geology
GA DG3AJ
UT WOS:000371941600008
ER
PT J
AU Graves, SJ
Asner, GP
Martin, RE
Anderson, CB
Colgan, MS
Kalantari, L
Bohlman, SA
AF Graves, Sarah J.
Asner, Gregory P.
Martin, Roberta E.
Anderson, Christopher B.
Colgan, Matthew S.
Kalantari, Leila
Bohlman, Stephanie A.
TI Tree Species Abundance Predictions in a Tropical Agricultural Landscape
with a Supervised Classification Model and Imbalanced Data
SO REMOTE SENSING
LA English
DT Article
DE Support Vector Machine; imaging spectroscopy; class imbalance; tropics;
agriculture; operational species mapping
ID SUPPORT VECTOR MACHINES; LIDAR DATA; IMAGING SPECTROSCOPY; ESTIMATING
AREA; LAND CHANGE; ACCURACY; BIODIVERSITY; IMAGERY; FUSION; ERROR
AB Mapping species through classification of imaging spectroscopy data is facilitating research to understand tree species distributions at increasingly greater spatial scales. Classification requires a dataset of field observations matched to the image, which will often reflect natural species distributions, resulting in an imbalanced dataset with many samples for common species and few samples for less common species. Despite the high prevalence of imbalanced datasets in multiclass species predictions, the effect on species prediction accuracy and landscape species abundance has not yet been quantified. First, we trained and assessed the accuracy of a support vector machine (SVM) model with a highly imbalanced dataset of 20 tropical species and one mixed-species class of 24 species identified in a hyperspectral image mosaic (350-2500 nm) of Panamanian farmland and secondary forest fragments. The model, with an overall accuracy of 62% +/- 2.3% and F-score of 59% +/- 2.7%, was applied to the full image mosaic (23,000 ha at a 2-m resolution) to produce a species prediction map, which suggested that this tropical agricultural landscape is more diverse than what has been presented in field-based studies. Second, we quantified the effect of class imbalance on model accuracy. Model assessment showed a trend where species with more samples were consistently over predicted while species with fewer samples were under predicted. Standardizing sample size reduced model accuracy, but also reduced the level of species over- and under-prediction. This study advances operational species mapping of diverse tropical landscapes by detailing the effect of imbalanced data on classification accuracy and providing estimates of tree species abundance in an agricultural landscape. Species maps using data and methods presented here can be used in landscape analyses of species distributions to understand human or environmental effects, in addition to focusing conservation efforts in areas with high tree cover and diversity.
C1 [Graves, Sarah J.; Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, POB 11041, Gainesville, FL 32611 USA.
[Asner, Gregory P.; Martin, Roberta E.; Anderson, Christopher B.; Colgan, Matthew S.] Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA.
[Kalantari, Leila] Univ Florida, Dept Comp & Informat Sci & Engn, POB 116120, Gainesville, FL 32611 USA.
[Bohlman, Stephanie A.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
RP Graves, SJ (reprint author), Univ Florida, Sch Forest Resources & Conservat, POB 11041, Gainesville, FL 32611 USA.
EM sjgraves@ufl.edu; gpa@carnegiescience.edu; rmartin@carnegiescience.edu;
cbanders@carnegiescience.edu; matthew.colgan@gmail.com;
leila@cise.ufl.edu; sbohlman@ufl.edu
OI Graves, Sarah/0000-0003-3805-4242
FU Grantham Foundation; Joshua C. Dickinson IV Fellowship; Tinker Travel
Fund through the University of Florida
FX The authors thank Jairo Batista Bernal, Diogenes Ibarra, Michelle
Goodfellow, Lesely Candaleria, and Luis Mancilla for assisting with data
collection in the field; the Azuero Earth Project for logistical
support; and Trevor Caughlin, Wendell Cropper, Francis Putz, and Sami
Rifai for guidance with this topic. The remote sensing data collection,
processing and analyses was supported by grants from the Grantham
Foundation for the Protection of the Environment and William R. Hearst
III. Funding for field data collection was provided by the Joshua C.
Dickinson IV Fellowship and the Tinker Travel Fund through the
University of Florida. The Carnegie Airborne Observatory is made
possible by the Avatar Alliance Foundation, John D. and Catherine T.
MacArthur Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr.,
and William R. Hearst III.
NR 58
TC 4
Z9 4
U1 12
U2 23
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2016
VL 8
IS 2
AR 161
DI 10.3390/rs8020161
PG 21
WC Remote Sensing
SC Remote Sensing
GA DG2LO
UT WOS:000371898800001
ER
PT J
AU Hedley, JD
Roelfsema, CM
Chollett, I
Harborne, AR
Heron, SF
Weeks, SJ
Skirving, WJ
Strong, AE
Eakin, CM
Christensen, TRL
Ticzon, V
Bejarano, S
Mumby, PJ
AF Hedley, John D.
Roelfsema, Chris M.
Chollett, Iliana
Harborne, Alastair R.
Heron, Scott F.
Weeks, Scarla J.
Skirving, William J.
Strong, Alan E.
Eakin, C. Mark
Christensen, Tyler R. L.
Ticzon, Victor
Bejarano, Sonia
Mumby, Peter J.
TI Remote Sensing of Coral Reefs for Monitoring and Management: A Review
SO REMOTE SENSING
LA English
DT Review
DE coral reef; management; monitoring; habitat; physical environment;
review
ID GREAT-BARRIER-REEF; FISH SPECIES RICHNESS; LANDSAT TM IMAGERY; TROPICAL
COASTAL RESOURCES; SEA-SURFACE TEMPERATURE; WATER COLUMN CORRECTION;
BISCAYNE NATIONAL-PARK; CO2 PARTIAL-PRESSURE; GULF-OF-MEXICO;
CLIMATE-CHANGE
AB Coral reefs are in decline worldwide and monitoring activities are important for assessing the impact of disturbance on reefs and tracking subsequent recovery or decline. Monitoring by field surveys provides accurate data but at highly localised scales and so is not cost-effective for reef scale monitoring at frequent time points. Remote sensing from satellites is an alternative and complementary approach. While remote sensing cannot provide the level of detail and accuracy at a single point than a field survey, the statistical power for inferring large scale patterns benefits in having complete areal coverage. This review considers the state of the art of coral reef remote sensing for the diverse range of objectives relevant for management, ranging from the composition of the reef: physical extent, benthic cover, bathymetry, rugosity; to environmental parameters: sea surface temperature, exposure, light, carbonate chemistry. In addition to updating previous reviews, here we also consider the capability to go beyond basic maps of habitats or environmental variables, to discuss concepts highly relevant to stakeholders, policy makers and public communication: such as biodiversity, environmental threat and ecosystem services. A clear conclusion of the review is that advances in both sensor technology and processing algorithms continue to drive forward remote sensing capability for coral reef mapping, particularly with respect to spatial resolution of maps, and synthesis across multiple data products. Both trends can be expected to continue.
C1 [Hedley, John D.] Environm Comp Sci Ltd, Raymond Penny House, Tiverton EX16 6LR, Devon, England.
[Roelfsema, Chris M.] Univ Queensland, Remote Sensing Res Ctr, Sch Geog Planning & Environm Management, Brisbane, Qld 4072, Australia.
[Chollett, Iliana] Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
[Harborne, Alastair R.; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Marine Spatial Ecol Lab, Brisbane, Qld 4072, Australia.
[Harborne, Alastair R.; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Australian Res Council Ctr Excellence Coral Reef, Brisbane, Qld 4072, Australia.
[Harborne, Alastair R.] Florida Int Univ, Dept Biol Sci, 3000 Northeast 151 St, North Miami, FL 33181 USA.
[Heron, Scott F.; Skirving, William J.; Strong, Alan E.; Eakin, C. Mark; Christensen, Tyler R. L.] NOAA, Coral Reef Watch, College Pk, MD 20740 USA.
[Heron, Scott F.; Skirving, William J.; Strong, Alan E.; Christensen, Tyler R. L.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA.
[Heron, Scott F.] James Cook Univ, Dept Phys, Marine Geophys Lab, Coll Sci Technol & Engn, Townsville, Qld 4811, Australia.
[Weeks, Scarla J.] Univ Queensland, Biophys Oceanog Grp, Remote Sensing Res Ctr, Sch Geog Planning & Environm Management, Brisbane, Qld 4072, Australia.
[Ticzon, Victor] Univ Philippines, Inst Biol Sci, Coll Arts & Sci, Los Banos Coll, Laguna 4031, Philippines.
[Bejarano, Sonia] Leibniz Ctr Trop Marine Ecol, Fahrenheitstr 6, D-28359 Bremen, Germany.
RP Hedley, JD (reprint author), Environm Comp Sci Ltd, Raymond Penny House, Tiverton EX16 6LR, Devon, England.
EM j.d.hedley@envirocs.com; c.roelfsema@uq.edu.au;
iliana.chollett@gmail.com; a.harborne@uq.edu.au; scott.heron@noaa.gov;
s.weeks@uq.edu.au; william.skirving@noaa.gov; alan.e.strong@noaa.gov;
mark.eakin@noaa.gov; trlchristensen@gmail.com; vsticzon@up.edu.ph;
sonia.bejarano@leibniz-zmt.de; p.j.mumby@uq.edu.au
RI Harborne, Alastair/F-6155-2013; Heron, Scott/E-7928-2011; Skirving,
William/E-7927-2011; Eakin, C. Mark/F-5585-2010; Bejarano,
Sonia/S-7784-2016
OI Harborne, Alastair/0000-0002-6818-8615; Skirving,
William/0000-0003-0167-6427; Bejarano, Sonia/0000-0001-6451-6354
FU Summit Foundation; Natural Environment Research Council, UK
[NE/F015704/1]; Australian Research Council [DE120102459]
FX This paper was initiated as part of the World Bank/GEF Coral Reef
Targeted Research and Capacity Building Program. The authors thank Andy
Hooten and Marea Hatziolos for making this collaboration possible. I.
Chollett is funded by the Summit Foundation and this is manuscript
contribution number 1021 from the Smithsonian Marine Station at Fort
Pierce, Florida. A. Harborne was funded by the Natural Environment
Research Council, UK (fellowship NE/F015704/1) and the Australian
Research Council (fellowship DE120102459). The contents in this
manuscript are solely the opinions of the authors and do not constitute
a statement of policy, decision or position on behalf of NOAA or the
U.S. Government.
NR 301
TC 4
Z9 4
U1 25
U2 58
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2016
VL 8
IS 2
AR 118
DI 10.3390/rs8020118
PG 40
WC Remote Sensing
SC Remote Sensing
GA DG2LO
UT WOS:000371898800067
ER
PT J
AU Nottingham, AT
Turner, BL
Whitaker, J
Ostle, N
Bardgett, RD
McNamara, NP
Salinas, N
Meir, P
AF Nottingham, Andrew T.
Turner, Benjamin L.
Whitaker, Jeanette
Ostle, Nick
Bardgett, Richard D.
McNamara, Niall P.
Salinas, Norma
Meir, Patrick
TI Temperature sensitivity of soil enzymes along an elevation gradient in
the Peruvian Andes
SO BIOGEOCHEMISTRY
LA English
DT Article
DE beta-glucosidase; beta-xylanase; Q(10) values; Soil carbon; Tropical
montane forest
ID MICROBIAL PROCESSES; THERMAL ADAPTATION; ORGANIC-CARBON; FOREST;
CLIMATE; DECOMPOSITION; AVAILABILITY; RESPIRATION; COMMUNITIES;
PEATLANDS
AB Soil enzymes are catalysts of organic matter depolymerisation, which is of critical importance for ecosystem carbon (C) cycling. Better understanding of the sensitivity of enzymes to temperature will enable improved predictions of climate change impacts on soil C stocks. These impacts may be especially large in tropical montane forests, which contain large amounts of soil C. We determined the temperature sensitivity (Q (10)) of a range of hydrolytic and oxidative enzymes involved in organic matter cycling from soils along a 1900 m elevation gradient (a 10 A degrees C mean annual temperature gradient) of tropical montane forest in the Peruvian Andes. We investigated whether the activity (V (max)) of selected enzymes: (i) exhibited a Q (10) that varied with elevation and/or soil properties; and (ii) varied among enzymes and according to the complexity of the target substrate for C-degrading enzymes. The Q (10) of V (max) for beta-glucosidase and beta-xylanase increased with increasing elevation and declining mean annual temperature. For all other enzymes, including cellobiohydrolase, N-acetyl beta-glucosaminidase and phosphomonoesterase, the Q (10) of V (max) did not vary linearly with elevation. Hydrolytic enzymes that degrade more complex C compounds had a greater Q (10) of V (max), but this pattern did not apply to oxidative enzymes because phenol oxidase had the lowest Q (10) value of all enzymes studied here. Our findings suggest that regional differences in the temperature sensitivities of different enzyme classes may influence the terrestrial C cycle under future climate warming.
C1 [Nottingham, Andrew T.; Meir, Patrick] Univ Edinburgh, Sch Geosci, Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland.
[Nottingham, Andrew T.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Nottingham, Andrew T.] Geography Bldg Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland.
[Whitaker, Jeanette; McNamara, Niall P.] Lancaster Environm Ctr, Ctr Ecol & Hydrol, Lib Ave, Lancaster LA1 4AP, England.
[Ostle, Nick] Univ Lancaster, Lancaster Environm Ctr, Lib Ave, Lancaster LA1 4YQ, England.
[Bardgett, Richard D.] Univ Manchester, Fac Life Sci, Michael Smith Bldg,Oxford Rd, Manchester M13 9PT, Lancs, England.
[Salinas, Norma] Pontificia Univ Catolica Peru, Secc Quim, Lima, Peru.
[Salinas, Norma] Environm Change Inst, Sch Geog & Environm, S Parks Rd, Oxford OX1 3QY, England.
[Meir, Patrick] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia.
RP Nottingham, AT (reprint author), Geography Bldg Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland.
EM anotting@staffmail.ed.ac.uk
RI Turner, Benjamin/E-5940-2011; McNamara, Niall/B-4907-2008; Whitaker,
Jeanette/A-9266-2013; Salinas, Norma/K-8960-2015; Ostle,
Nicholas/E-4847-2014
OI Turner, Benjamin/0000-0002-6585-0722; Whitaker,
Jeanette/0000-0001-8824-471X; Salinas, Norma/0000-0001-9941-2109; Ostle,
Nicholas/0000-0003-3263-3702
FU UK Natural Environment Research Council (NERC) [NE/G018278/1,
NE/F002149/1]; ARC [FT110100457]; European Union [FP7-2012-329360]
FX This study is a product of the Andes Biodiversity and Ecosystem Research
Group consortium (www.andesconservation.org) and was financed by the UK
Natural Environment Research Council (NERC) (grant numbers NE/G018278/1,
NE/F002149/1), and also supported by ARC grant FT110100457 to PM and a
European Union Marie-Curie Fellowship FP7-2012-329360 to ATN. We thank
the Asociacion para la Conservacion de la Cuenca Amazonica (ACCA) in
Cusco and the Instituto Nacional de Recursos Naturales (INRENA) in Lima
for access to the study sites. For their logistical support we thank Dr.
Eric Cosio and Eliana Esparza Ballon at Pontificia Universidad Catolica
del Peru (PUCP). For their support in the laboratory we thank Tania
Romero and Dayana Agudo. For their support in the field we thank Adan
J.Q. Ccahuana, Walter H. Huasco, Javier E. S. Espejo and many others too
numerous to mention here.
NR 60
TC 2
Z9 2
U1 21
U2 39
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
EI 1573-515X
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD FEB
PY 2016
VL 127
IS 2-3
BP 217
EP 230
DI 10.1007/s10533-015-0176-2
PG 14
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DF8KH
UT WOS:000371606000005
ER
PT J
AU Gardner, JR
Fisher, TR
Jordan, TE
Knee, KL
AF Gardner, John R.
Fisher, Thomas R.
Jordan, Thomas E.
Knee, Karen L.
TI Balancing watershed nitrogen budgets: accounting for biogenic gases in
streams
SO BIOGEOCHEMISTRY
LA English
DT Article
DE Denitrification; Greenhouse gases; Headwater streams; Nitrogen; Radon;
Watershed budget
ID COASTAL MARINE ECOSYSTEMS; WHOLE-REACH SCALE; OXIDE PRODUCTION;
CHESAPEAKE BAY; PLAINS RIVER; DENITRIFICATION RATES; AQUATIC ECOSYSTEMS;
NORTHEASTERN USA; FRESH-WATER; EMISSIONS
AB Denitrification is critical for removal of reactive nitrogen (Nr) from ecosystems. However, measuring realistic, scalable rates and understanding the role of denitrification and other dissimilatory processes in watershed nitrogen (N) budgets remains a significant challenge in biogeochemistry. In this study, we focused on the stream reach and network scale in three Mid-Atlantic coastal plain watersheds. We applied open channel methods to measure biogenic N-2 and N2O gas fluxes derived from both in-stream and terrestrial nitrogen processing. A large portion of biogenic N-2 flux through streams (33-100 %, mean = 74 %) was a result of groundwater delivery of biogenic N-2 with the remaining portion due to in-stream N-2 production. In contrast, N2O was largely produced in-stream, with groundwater delivery contributing on average 12 % of the total biogenic N2O flux. We scaled these measurements across one stream network and compared them to hydrologic Nr export and net anthropogenic N inputs (NANI) to a 4.8 km(2) watershed. The N budget revealed that, during the study period, the biogenic N-2 flux through streams was comparable to the difference between NANI and hydrologic Nr export (i.e. the "missing" N). This study provides a methodological and conceptual framework for incorporating terrestrial and in-stream derived biogenic N gas fluxes into watershed N budgets and supports the hypothesis that denitrification is the primary fate of NANI that is not exported in streamflow.
C1 [Gardner, John R.; Fisher, Thomas R.] Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD USA.
[Jordan, Thomas E.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
[Knee, Karen L.] Amer Univ, Dept Environm Sci, Washington, DC 20016 USA.
[Gardner, John R.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
RP Gardner, JR (reprint author), Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD USA.; Gardner, JR (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
EM john.r.gardner@duke.edu
FU NSF (DEB) [0919181, 0919141, 1252923]; Maryland Water Resources Research
Center; Izaak Walton League-Midshore Chapter; Horn Point Laboratory
Graduate Student Fellowship
FX We thank the members of the Fisher lab group (Anne Gustafson, Rebecca
Fox, Dana Bunnell-Young, Keota Silaphone, and Lindsay Tempison) and Todd
Kana at the Horn Point Laboratory for their support. The following
people from the Jordan lab group at Smithsonian Environmental Research
Center provided field and lab assistance: Joe Miklas, Jake Wilhelm, and
Carey Pelc. We thank Keith Eshleman for comments that led to the
improvement of the manuscript. Funding sources include NSF (DEB#
0919181, DEB#0919141, DEB #1252923), Maryland Water Resources Research
Center, Izaak Walton League-Midshore Chapter, and a Horn Point
Laboratory Graduate Student Fellowship.
NR 89
TC 2
Z9 2
U1 9
U2 25
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
EI 1573-515X
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD FEB
PY 2016
VL 127
IS 2-3
BP 231
EP 253
DI 10.1007/s10533-015-0177-1
PG 23
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DF8KH
UT WOS:000371606000006
ER
PT J
AU Danehkar, A
Parker, QA
Steffen, W
AF Danehkar, A.
Parker, Q. A.
Steffen, W.
TI FAST, LOW-IONIZATION EMISSION REGIONS OF THE PLANETARY NEBULA M2-42
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE ISM: jets and outflows; planetary nebulae: individual (M2-42); stars:
evolution
ID FIELD SPECTROGRAPH WIFES; CENTRAL STARS; WOLF-RAYET; GALACTIC BULGE;
QUANTITATIVE CLASSIFICATION; ELEMENTAL ABUNDANCES; CATALOG;
MICROSTRUCTURES; KINEMATICS; EXCITATION
AB Spatially resolved observations of the planetary nebula M2-42 (PN G008.2-04.8) obtained with the Wide Field Spectrograph on the Australian National University 2.3 m telescope have revealed the remarkable features of bipolar collimated jets emerging from its main structure. Velocity-resolved channel maps derived from the [N II]gimel 6584 emission line disentangle different morphological components of the nebula. This information is used to develop a three-dimensional morpho-kinematic model, which consists of an equatorial dense torus and a pair of asymmetric bipolar outflows. The expansion velocity of about 20 km s(-1) is measured from the spectrum integrated over the main shell. However, the deprojected velocities of the jets are found to be in the range of 80-160 km s(-1) with respect to the nebular center. It is found that the mean density of the collimated outflows, 595 +/- 125 cm(-3), is five times lower than that of the main shell, 3150 cm(-3), whereas their singly ionized nitrogen and sulfur abundances are about three times higher than those determined from the dense shell. The results indicate that the features of the collimated jets are typical of fast, low-ionization emission regions.
C1 [Danehkar, A.; Parker, Q. A.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Danehkar, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Parker, Q. A.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Parker, Q. A.] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
[Steffen, W.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico.
RP Danehkar, A (reprint author), Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.; Danehkar, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ashkbiz.danehkar@cfa.harvard.edu
RI Danehkar, Ashkbiz/C-2053-2009
OI Danehkar, Ashkbiz/0000-0003-4552-5997
FU Macquarie University; Australian Astronomical Observatory (AAO); ESO
Survey programme [179.B-2002]; [UNAM-PAPIIT 101014]
FX A.D. acknowledges the award of a Research Excellence Scholarship from
Macquarie University. Q.A.P. acknowledges support from Macquarie
University and the Australian Astronomical Observatory (AAO). W.S.
acknowledges support from grant UNAM-PAPIIT 101014. We would like to
thank the staff at the ANU Siding Spring Observatory for their support.
We acknowledge use of data from the VISTA telescope under ESO Survey
programme ID 179.B-2002. We thank the anonymous referee whose
suggestions and comments have greatly improved the paper.
NR 47
TC 2
Z9 2
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2016
VL 151
IS 2
AR 38
DI 10.3847/0004-6256/151/2/38
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF3MO
UT WOS:000371248600018
ER
PT J
AU Dawson, KS
Kneib, JP
Percival, WJ
Alam, S
Albareti, FD
Anderson, SF
Armengaud, E
Aubourg, E
Bailey, S
Bautista, JE
Berlind, AA
Bershady, MA
Beutler, F
Bizyaev, D
Blanton, MR
Blomqvist, M
Bolton, AS
Boyy, J
Brandt, WN
Brinkmann, J
Brownstein, JR
Burtin, E
Busca, NG
Cai, Z
Chuang, CH
Clerc, N
Comparat, J
Cope, F
Croft, RAC
Cruz-Gonzalez, I
da Costa, LN
Cousinou, MC
Darling, J
de la Macorra, A
de la Torre, S
Delubac, T
des Bourboux, HD
Dwelly, T
Ealet, A
Eisenstein, DJ
Eracleous, M
Escoffier, S
Fan, XH
Finoguenov, A
Font-Ribera, A
Frinchaboy, P
Gaulme, P
Georgakakis, A
Green, P
Guo, H
Guy, J
Ho, S
Holder, D
Huehnerhoff, J
Hutchinson, T
Jing, YP
Jullo, E
Kamble, V
Kinemuchi, K
Kirkby, D
Kitaura, FS
Klaene, MA
Laher, RR
Lang, D
Laurent, P
Le Goff, JM
Li, C
Liang, Y
Lima, M
Lin, Q
Lin, W
Lin, YT
Long, DC
Lundgren, B
MacDonald, N
Maia, MAG
Malanushenko, E
Malanushenko, V
Mariappan, V
McBride, CK
McGreer, ID
Menard, B
Merloni, A
Meza, A
Montero-Dorta, AD
Muna, D
Myers, AD
Nandra, K
Naugle, T
Newman, JA
Noterdaeme, P
Nugent, P
Ogando, N
Olmstead, MD
Oravetz, A
Oravetz, DJ
Padmanabhan, N
Palanque-Delabrouille, N
Pan, K
Parejko, JK
Paris, I
Peacock, JA
Petitjean, P
Pieri, MM
Pisani, A
Prada, F
Prakash, A
Raichoor, A
Reid, B
Rich, J
Ridl, J
Rodriguez-Torres, S
Rosell, AC
Ross, AJ
Rossi, G
Ruan, J
Salvato, M
Sayres, C
Schneider, DP
Schlegel, DJ
Seljak, U
Seo, HJ
Sesar, B
Shandera, S
Shu, YP
Slosar, A
Sobreira, F
Streblyanska, A
Suzuki, N
Taylor, D
Tao, C
Tinker, JL
Tojeiro, R
Vargas-Magana, M
Wang, YT
Weaver, BA
Weinberg, DH
White, M
Wood-Vasey, WM
Yeche, C
Zhai, ZX
Zhao, C
Zhao, GB
Zheng, Z
Zhu,GB
Zou, H
AF Dawson, Kyle S.
Kneib, Jean -Paul
Percival, Will J.
Alam, Shadab
Albareti, Franco D.
Anderson, Scott F.
Armengaud, Eric
Aubourg, Eric
Bailey, Stephen
Bautista, Julian E.
Berlind, Andreas A.
Bershady, Matthew A.
Beutler, Florian
Bizyaev, Dmitry
Blanton, Michael R.
Blomqvist, Michael
Bolton, Adam S.
Boyy, Jo
Brandt, W. N.
Brinkmann, Jon
Brownstein, Joel R.
Burtin, Etienne
Busca, N. G.
Cai, Zheng
Chuang, Chia-Hsun
Clerc, Nicolas
Comparat, Johan
Cope, Frances
Croft, Rupert A. C.
Cruz-Gonzalez, Irene
da Costa, Lutz N.
Cousinou, Marie-Claude
Darling, Jeremy
de la Macorra, Axel
de la Torre, Sylvain
Delubac, Timothee
des Bourboux, Helion du Mas
Dwelly, Tom
Ealet, Anne
Eisenstein, Daniel J.
Eracleous, Michael
Escoffier, S.
Fan, Xiaohui
Finoguenov, Alexis
Font-Ribera, Andreu
Frinchaboy, Peter
Gaulme, Patrick
Georgakakis, Antonis
Green, Paul
Guo, Hong
Guy, Julien
Ho, Shirley
Holder, Diana
Huehnerhoff, Joe
Hutchinson, Timothy
Jing, Yipeng
Jullo, Eric
Kamble, Vikrant
Kinemuchi, Karen
Kirkby, David
Kitaura, Francisco-Shu
Klaene, Mark A.
Laher, Russ R.
Lang, Dustin
Laurent, Pierre
Le Goff, Jean-Marc
Li, Cheng
Liang, Yu
Lima, Marcos
Lin, Qiufan
Lin, Weipeng
Lin, Yen-Ting
Long, Daniel C.
Lundgren, Britt
MacDonald, Nicholas
Maia, Marcio Antonio Geimba
Malanushenko, Elena
Malanushenko, Viktor
Mariappan, Vivek
McBride, Cameron K.
McGreer, Ian D.
Menard, Brice
Merloni, Andrea
Meza, Andres
Montero-Dorta, Antonio D.
Muna, Demitri
Myers, Adam D.
Nandra, Kirpal
Naugle, Tracy
Newman, Jeffrey A.
Noterdaeme, Pasquier
Nugent, Peter
Ogando, Nugentricardo
Olmstead, Matthew D.
Oravetz, Audrey
Oravetz, Daniel J.
Padmanabhan, Nikhil
Palanque-Delabrouille, Nathalie
Pan, Kaike
Parejko, John K.
Paris, Isabelle
Peacock, John A.
Petitjean, Patrick
Pieri, Matthew M.
Pisani, Alice
Prada, Francisco
Prakash, Abhishek
Raichoor, Anand
Reid, Beth
Rich, James
Ridl, Jethro
Rodriguez-Torres, Sergio
Rosell, Aurelio Carnero
Ross, Ashley J.
Rossi, Graziano
Ruan, John
Salvato, Mara
Sayres, Conor
Schneider, Donald P.
Schlegel, David J.
Seljak, Uros
Seo, Hee-Jong
Sesar, Branimir
Shandera, Sarah
Shu, Yiping
Slosar, Anze
Sobreira, Flavia
Streblyanska, Alina
Suzuki, Nao
Taylor, Donna
Tao, Charling
Tinker, Jeremy L.
Tojeiro, Rita
Vargas-Magana, Mariana
Wang, Yuting
Weaver, Benjamin A.
Weinberg, David H.
White, Martin
Wood-Vasey, W. M.
Yeche, Christophe
Zhai, Zhongxu
Zhao, Cheng
Zhao, Gong-bo
Zheng, Zheng
Zhu, Guangtun Ben
Zou, Hu
TI THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW
AND EARLY DATA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology: observations; surveys
ID DIGITAL SKY SURVEY; DATA RELEASE 9; REDSHIFT-SPACE DISTORTIONS; LY-ALPHA
FOREST; PHOTOMETRICALLY CLASSIFIED QUASARS; PRIMORDIAL NON-GAUSSIANITY;
SUPERNOVA LEGACY SURVEY; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE;
DR11 BOSS GALAXIES
AB In a six-year program started in 2014 July, the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) will conduct novel cosmological observations using the BOSS spectrograph at Apache Point Observatory. These observations will be conducted simultaneously with the Time Domain Spectroscopic Survey (TDSS) designed for variability studies and the Spectroscopic Identification of eROSITA Sources (SPIDERS) program designed for studies of X-ray sources. In particular, eBOSS will measure with percent-level precision the distance-redshift relation with baryon acoustic oscillations (BAO) in the clustering of matter. eBOSS will use four different tracers of the underlying matter density field to vastly expand the volume covered by BOSS and map the large-scale-structures over the relatively unconstrained redshift range 0.6 < z < 2.2. Using more than 250,000 new, spectroscopically confirmed luminous red galaxies at a median redshift z = 0.72, we project that eBOSS will yield measurements of the angular diameter distance d(A)(z) to an accuracy of 1.2% and measurements of H(z) to 2.1% when combined with the z > 0.6 sample of BOSS galaxies. With similar to 195,000 new emission line galaxy redshifts, we expect BAO measurements of d(A)(z) to an accuracy of 3.1% and H(z) to 4.7% at an effective redshift of z = 0.87. A sample of more than 500,000 spectroscopically confirmed quasars will provide the first BAO distance measurements over the redshift range 0.9 < z < 2.2, with expected precision of 2.8% and 4.2% on d(A)(z) and H(z), respectively. Finally, with 60,000 new quasars and re-observation of 60,000 BOSS quasars, we will obtain new Lya forest measurements at redshifts z > 2.1; these new data will enhance the precision of d(A)(z) and H(z) at z > 2.1 by a factor of 1.44 relative to BOSS. Furthermore, eBOSS will provide improved tests of General Relativity on cosmological scales through redshift-space distortion measurements, improved tests for non-Gaussianity in the primordial density field, and new constraints on the summed mass of all neutrino species. Here, we provide an overview of the cosmological goals, spectroscopic target sample, demonstration of spectral quality from early data, and projected cosmological constraints from eBOSS.
C1 [Dawson, Kyle S.; Bautista, Julian E.; Bolton, Adam S.; Brownstein, Joel R.; Guo, Hong; Hutchinson, Timothy; Kamble, Vikrant; Mariappan, Vivek; Montero-Dorta, Antonio D.; Shu, Yiping; Taylor, Donna; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kneib, Jean -Paul; Delubac, Timothee] Ecole Polytech Fed Lausanne, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, Switzerland.
[Kneib, Jean -Paul; de la Torre, Sylvain; Jullo, Eric; Pieri, Matthew M.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Percival, Will J.; Ross, Ashley J.; Tojeiro, Rita; Wang, Yuting; Zhao, Gong-bo] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England.
[Alam, Shadab; Croft, Rupert A. C.; Ho, Shirley; Lang, Dustin] Carnegie Mellon Univ, Dept Phys, Bruce & Astrid McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
[Albareti, Franco D.; Chuang, Chia-Hsun; Comparat, Johan; Prada, Francisco; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain.
[Anderson, Scott F.; MacDonald, Nicholas; Ruan, John; Sayres, Conor] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Armengaud, Eric; Burtin, Etienne; des Bourboux, Helion du Mas; Laurent, Pierre; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Raichoor, Anand; Rich, James; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France.
[Aubourg, Eric; Busca, N. G.] Univ Paris Diderot, APC, CNRS IN2P3, CEA IRFU,Observ Paris,Sorbonne Paris Cite, Paris, France.
[Bailey, Stephen; Beutler, Florian; Font-Ribera, Andreu; Nugent, Peter; Reid, Beth; Schlegel, David J.; Seljak, Uros; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, One Cyclotron Rd, Berkeley, CA 94720 USA.
[Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, PMB 401807,2401 Vanderbilt Pl, Nashville, TN 37240 USA.
[Bershady, Matthew A.; Lundgren, Britt] Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53703 USA.
[Bizyaev, Dmitry; Bolton, Adam S.; Brinkmann, Jon; Cope, Frances; Gaulme, Patrick; Holder, Diana; Huehnerhoff, Joe; Kinemuchi, Karen; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Naugle, Tracy; Oravetz, Audrey; Oravetz, Daniel J.; Pan, Kaike] Apache Point Observ, POB 59, Sunspot, NM 88349 USA.
[Bizyaev, Dmitry; Kinemuchi, Karen; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Audrey; Oravetz, Daniel J.; Pan, Kaike] New Mexico State Univ, Dept Astron, MSC 4500,POB 30001, Las Cruces, NM 88003 USA.
[Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia.
[Blanton, Michael R.; Tinker, Jeremy L.; Weaver, Benjamin A.; Zhai, Zhongxu] NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[Blomqvist, Michael; Kirkby, David] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Boyy, Jo] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Brandt, W. N.; Eracleous, Michael; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Eracleous, Michael; Schneider, Donald P.; Shandera, Sarah] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.; Eracleous, Michael] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Cai, Zheng; Fan, Xiaohui; McGreer, Ian D.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Clerc, Nicolas; Dwelly, Tom; Georgakakis, Antonis; Merloni, Andrea; Nandra, Kirpal; Ridl, Jethro; Salvato, Mara] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Cruz-Gonzalez, Irene; de la Macorra, Axel] Univ Autonoma Madrid, Inst Astron, AP 70-264, E-28049 Madrid, Spain.
[da Costa, Lutz N.; Maia, Marcio Antonio Geimba; Ogando, Nugentricardo; Rosell, Aurelio Carnero] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[da Costa, Lutz N.; Lima, Marcos; Maia, Marcio Antonio Geimba; Ogando, Nugentricardo; Rosell, Aurelio Carnero; Sobreira, Flavia] LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Cousinou, Marie-Claude; Ealet, Anne; Escoffier, S.; Pisani, Alice; Tao, Charling] Aix Marseille Univ, CNRS, IN2P3, CPPM UMR 7346, F-13288 Marseille, France.
[Darling, Jeremy] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
[Eisenstein, Daniel J.; Green, Paul; McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Finoguenov, Alexis] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, FI-00014 Helsinki, Finland.
[Frinchaboy, Peter] Texas Christian Univ, Dept Phys & Astron, 2800 South Univ Dr, Ft Worth, TX 76129 USA.
[Guo, Hong; Li, Cheng; Lin, Weipeng] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China.
[Guy, Julien] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, 4 Pl Jussieu, F-75252 Paris, France.
[Jing, Yipeng] Shanghai Jiao Tong Univ, Dept Phys & Astron, IFSA Collaborat Innovat Ctr, Shanghai 200240, Peoples R China.
[Kitaura, Francisco-Shu] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Laher, Russ R.] CALTECH, Spitzer Sci Ctr, M-S 314-6, Pasadena, CA 91125 USA.
[Liang, Yu; Lin, Qiufan; Tao, Charling; Zhao, Cheng] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China.
[Lima, Marcos] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Lin, Weipeng] Sun Yat Sen Univ, Sch Astron & Space Sci, Guangzhou 510275, Guangdong, Peoples R China.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Menard, Brice; Zhu, Guangtun Ben] Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, 3400 North Charles St, Baltimore, MD 21218 USA.
[Menard, Brice; Suzuki, Nao] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Meza, Andres] Univ Andres Bello, Dept Ciencias Fis, Ave Republ 220, Santiago, Chile.
[Muna, Demitri] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Muna, Demitri] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Newman, Jeffrey A.; Prakash, Abhishek; Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, Jeffrey A.; Prakash, Abhishek; Wood-Vasey, W. M.] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA.
[Noterdaeme, Pasquier; Petitjean, Patrick; Pisani, Alice] UPMC, CNRS, UMR7095, Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France.
[Nugent, Peter; Seljak, Uros; White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Olmstead, Matthew D.] Kings Coll, Dept Chem & Phys, Wilkes Barre, PA 18711 USA.
[Padmanabhan, Nikhil; Parejko, John K.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Paris, Isabelle] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy.
[Peacock, John A.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Pisani, Alice] Univ Paris 06, Sorbonne univ, UMR7095, Inst Astrophys Paris, 98Bis Bd Arago, F-75014 Paris, France.
[Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain.
[Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Ross, Ashley J.; Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea.
[Seljak, Uros; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Seljak, Uros] LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Seljak, Uros] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, Clippinger Labs 251B, Athens, OH 45701 USA.
[Sesar, Branimir] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Slosar, Anze] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA.
[Sobreira, Flavia] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Streblyanska, Alina] Inst Astrofis Canarias, C Via Lactea S-N, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Streblyanska, Alina] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Apdo Postal 20-364, Mexico City 01000, DF, Mexico.
[Wang, Yuting; Zhao, Gong-bo; Zou, Hu] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
RP Dawson, KS (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
EM kdawson@astro.utah.edu
RI Guo, Hong/J-5797-2015; Lima, Marcos/E-8378-2010; White,
Martin/I-3880-2015; Sobreira, Flavia/F-4168-2015; Croft,
Rupert/N-8707-2014; Georgakakis, Antonis/K-4457-2013; Jullo,
Eric/N-8351-2015;
OI Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070;
Sobreira, Flavia/0000-0002-7822-0658; Croft, Rupert/0000-0003-0697-2583;
Kirkby, David/0000-0002-8828-5463; Meza, Andres/0000-0002-9460-7828;
Jullo, Eric/0000-0002-9253-053X; Beutler, Florian/0000-0003-0467-5438;
Georgakakis, Antonis/0000-0002-3514-2442
FU U.S. Department of Energy [DE-SC000995]; ERC advanced grant LIDA; UK
STFC [ST/K0090X/1]; European Research Council through grant Darksurvey;
Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science
FX K.D. acknowledges support from the U.S. Department of Energy under Grant
DE-SC000995. J.P.K. and T.D. acknowledge support from the ERC advanced
grant LIDA. W.J.P. acknowledges support from the UK STFC through the
consolidated grant ST/K0090X/1, and from the European Research Council
through grant Darksurvey. This paper includes targets derived from the
images of the Wide-Field Infrared Survey Explorer, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration.r This paper represents an
effort by both the SDSS-III and SDSS-IV collaborations. Funding for
SDSS-III was provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. Funding for the Sloan
Digital Sky Survey IV has been provided by the Alfred P. Sloan
Foundation, the U.S. Department of Energy Office of Science, and the
Participating Institutions. SDSS-IV acknowledges support and resources
from the Center for High-Performance Computing at the University of
Utah. The SDSS web site is www.sdss.org.
NR 155
TC 38
Z9 38
U1 13
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2016
VL 151
IS 2
AR 44
DI 10.3847/0004-6256/151/2/44
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF3MO
UT WOS:000371248600024
ER
PT J
AU Eastman, JD
Beatty, TG
Siverd, RJ
Antognino, JMO
Penny, MT
Gonzales, EJ
Crepp, JR
Howard, AW
Avril, RL
Bieryla, A
Collins, K
Fulton, BJ
Ge, J
Gregorio, J
Ma, B
Mellon, SN
Oberst, TE
Wang, J
Gaudi, BS
Pepper, J
Stassun, KG
Buchhave, LA
Jensen, ELN
Latham, DW
Berlind, P
Calkins, ML
Cargile, PA
Colon, KD
Dhital, S
Esquerd, GA
Johnson, JA
Kielkopf, JF
Manner, M
Mao, QQ
McLeod, KK
Penev, K
Stefanik, RP
Street, R
Zambelli, R
DePoy, DL
Gould, A
Marshall, JL
Pogge, RW
Trueblood, M
Trueblood, P
AF Eastman, Jason D.
Beatty, Thomas G.
Siverd, Robert J.
Antognino, Joseph M. O.
Penny, Matthew T.
Gonzales, Erica J.
Crepp, Justin R.
Howard, Andrew W.
Avril, Ryan L.
Bieryla, Allyson
Collins, Karen
Fulton, Benjamin J.
Ge, Jian
Gregorio, Joao
Ma, Bo
Mellon, Samuel N.
Oberst, Thomas E.
Wang, Ji
Gaudi, B. Scott
Pepper, Joshua
Stassun, Keivan G.
Buchhave, Lars A.
Jensen, Eric L. N.
Latham, David W.
Berlind, Perry
Calkins, Michael L.
Cargile, Phillip A.
Colon, Knicole D.
Dhital, Saurav
Esquerd, Gilbert A.
Johnson, John Asher
Kielkopf, John F.
Manner, Mark
Mao, Qingqing
McLeod, Kim K.
Penev, Kaloyan
Stefanik, Robert P.
Street, Rachel
Zambelli, Roberto
DePoy, D. L.
Gould, Andrew
Marshall, Jennifer L.
Pogge, Richard W.
Trueblood, Mark
Trueblood, Patricia
TI KELT-4Ab: AN INFLATED HOT JUPITER TRANSITING THE BRIGHT (V similar to
10) COMPONENT OF A HIERARCHICAL TRIPLE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: visual; eclipses; planets and satellites: detection; planets
and satellites: dynamical evolution and stability; planets and
satellites: gaseous planets; techniques: photometric
ID DOUBLE STAR CATALOG; PLANET HD 149026B; STELLAR EVOLUTION; QUADRUPLE
SYSTEMS; MASS COMPANION; Y-2 ISOCHRONES; GIANT PLANETS; LIGHT CURVES;
EXOPLANETS; TELESCOPE
AB We report the discovery of KELT-4Ab, an inflated, transiting Hot Jupiter orbiting the brightest component of a hierarchical triple stellar system. The host star is an F star with T-eff = 6206 +/- 75 K, log g = 4.108 +/- 0.014, [Fe/H] = -0.116(-0.069)(+0.065), M-* = 1.201(-0.061)(+0.067) M-circle dot, and R-* = 1.603(-0.038)(+0.039) R-circle dot. The best-fit linear ephemeris is BJD(TDB) = 2456193.29157 +/- 0.00021 + E(2.9895936 +/- 0.0000048). With a magnitude of V similar to 10, a planetary radius of 1.699(-0.045)(+0.046) R-J, and a mass of 0.902(-0.059)(+0.060) M-J, it is the brightest host among the population of inflated Hot Jupiters (R-P > 1.5R(J)), making it a valuable discovery for probing the nature of inflated planets. In addition, its existence within a hierarchical triple and its proximity to Earth ( 210 pc) provide a unique opportunity for dynamical studies with continued monitoring with high resolution imaging and precision radial velocities. The projected separation between KELT-4A and KELT-4BC is 328 +/- 16 AU and the projected separation between KELT-4B and KELT-4C is 10.30 +/- 0.74 AU. Assuming face-on, circular orbits, their respective periods would be 3780 +/- 290 and 29.4 +/- 3.6 years and the astrometric motions relative to the epoch in this work of both the binary stars around each other and of the binary around the primary star would be detectable now and may provide meaningful constraints on the dynamics of the system.
C1 [Eastman, Jason D.; Bieryla, Allyson; Buchhave, Lars A.; Latham, David W.; Berlind, Perry; Calkins, Michael L.; Cargile, Phillip A.; Esquerd, Gilbert A.; Johnson, John Asher; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA.
[Siverd, Robert J.; Street, Rachel] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
[Antognino, Joseph M. O.; Penny, Matthew T.; Gaudi, B. Scott; Gould, Andrew; Pogge, Richard W.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Gonzales, Erica J.; Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Howard, Andrew W.; Fulton, Benjamin J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Avril, Ryan L.; Mellon, Samuel N.; Oberst, Thomas E.] Westminster Coll, Dept Phys, New Wilmington, PA 16172 USA.
[Collins, Karen; Stassun, Keivan G.; Mao, Qingqing] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Ge, Jian; Ma, Bo] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Gregorio, Joao] Atalaia Grp & Crow Observ, Portalegre, Portugal.
[Mellon, Samuel N.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Wang, Ji] CALTECH, Dept Astrophys, MC 249-17, Pasadena, CA 91125 USA.
[Pepper, Joshua; Colon, Knicole D.] Lehigh Univ, Dept Phys, Bldg 16, Bethlehem, PA 18015 USA.
[Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Colon, Knicole D.] NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA.
[Colon, Knicole D.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA.
[Dhital, Saurav] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Kielkopf, John F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA.
[Manner, Mark] Spot Observ, Nunnelly, TN 37137 USA.
[McLeod, Kim K.] Wellesley Coll, Wellesley, MA 02481 USA.
[Penev, Kaloyan] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Zambelli, Roberto] Soc Astronom Lunae, Via Montefrancio 77, I-19030 Castelnuovo Magra, Italy.
[DePoy, D. L.; Marshall, Jennifer L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Marshall, Jennifer L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Trueblood, Mark; Trueblood, Patricia] Winer Observ, Sonoita, AZ 85637 USA.
RP Eastman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Jensen, Eric/0000-0002-4625-7333; Pepper, Joshua/0000-0002-3827-8417
FU NASA [NNG04GO70G]; NSF CAREER [AST-1056524]; NASA Kentucky Space Grant
Consortium Graduate Fellowship; Vanderbilt Office of the Provost through
the Vanderbilt Initiative in Data-intensive Astrophysics; National
Science Foundation [AST-0849736, AST-1009810]; Kepler Mission through
NASA Cooperative Agreement [NNX11AB99A]; Smithsonian Astrophysical
Observatory; NSF [1313252, AST-0705139]; University of Florida; National
Science Foundation Graduate Research Fellowship [2014184874]; National
Aeronautics and Space Administration; National Science Foundation
FX We extend special thanks to those of Hawaiian ancestry on whose sacred
mountain of Mauna Kea we are privileged to be guests. Without their
generous hospitality, the Keck observations presented herein would not
have been possible. Early work on KELT-North was supported by NASA Grant
NNG04GO70G. Work by B.S.G., J.D.E., and T.G.B. was partially supported
by NSF CAREER Grant AST-1056524. K.A.C. was supported by a NASA Kentucky
Space Grant Consortium Graduate Fellowship. J.A.P. and K.G.S.
acknowledge support from the Vanderbilt Office of the Provost through
the Vanderbilt Initiative in Data-intensive Astrophysics. K.G.S. and
L.H. acknowledge the support of the National Science Foundation through
PAARE grant AST-0849736 and AAG grant AST-1009810. The TRES and
KeplerCam observations were obtained with partial support from the
Kepler Mission through NASA Cooperative Agreement NNX11AB99A with the
Smithsonian Astrophysical Observatory, D.W.L. PI. J.M.O.A. is supported
in part by NSF Award #1313252. J.G., B.M., and J.W. acknowledge support
from NSF AST-0705139 and the University of Florida for the development
of the EXPERT instrument and observations. This material is based upon
work supported by the National Science Foundation Graduate Research
Fellowship under grant No. 2014184874. Any opinion, findings, and
conclusions or recommendations expressed in this material are those of
the authors(s) and do not necessarily reflect the views of the National
Science Foundation.; This publication makes use of data products from
the Two Micron All Sky Survey, which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation.
NR 102
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2016
VL 151
IS 2
AR 45
DI 10.3847/0004-6256/151/2/45
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF3MO
UT WOS:000371248600025
ER
PT J
AU Cao, C
Xu, CK
Domingue, D
Buat, V
Cheng, YW
Gao, Y
Huang, JS
Jarrett, TH
Lisenfeld, U
Lu, NY
Mazzarella, J
Sun, WH
Wu, H
Yun, MS
Ronca, J
Jacques, A
AF Cao, Chen
Xu, Cong Kevin
Domingue, Donovan
Buat, Veronique
Cheng, Yi-Wen
Gao, Yu
Huang, Jiasheng
Jarrett, Thomas H.
Lisenfeld, Ute
Lu, Nanyao
Mazzarella, Joe
Sun, Wei-Hsin
Wu, Hong
Yun, Min S.
Ronca, Joseph
Jacques, Allison
TI HERSCHEL OBSERVATIONS OF MAJOR MERGER PAIRS AT z=0: DUST MASS AND STAR
FORMATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: interactions;
galaxies: starburst
ID DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL
ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; INTERACTING GALAXIES;
FORMATION RATES; METALLICITY RELATION; FORMING GALAXIES; COSMIC
EVOLUTION; BINARY GALAXIES
AB We present Herschel PACS and SPIRE far-infrared (FIR) and submillimeter imaging observations for a large K-band selected sample of 88 close major-merger pairs of galaxies (H-KPAIRs) in 6 photometric bands (70, 100, 160, 250, 350, and 500 mu m). Among 132 spiral galaxies in the 44 spiral-spiral (S+S) pairs and 44 spiral-elliptical (S+ E) pairs, 113 are detected in at least 1 Herschel band. The star formation rate (SFR) and dust mass (M-dust) are derived from the IR SED fitting. The mass of total gas (M-gas) is estimated by assuming a constant dust-to-gas mass ratio of 0.01. Star-forming spiral galaxies (SFGs) in S+ S pairs show significant enhancements in both specific star formation rate (sSFR) and star formation efficiency (SFE), while having nearly the same gas mass compared to control galaxies. On the other hand, for SFGs in S+ E pairs, there is no significant sSFR enhancement and the mean SFE enhancement is significantly lower than that of SFGs in S+ S pairs. This suggests an important role for the disk-disk collision in the interaction-induced star formation. The M-gas of SFGs in S+ E pairs is marginally lower than that of their counterparts in both S+ S pairs and the control sample. Paired galaxies with and without interaction signs do not differ significantly in their mean sSFR and SFE. As found in previous works, this much larger sample confirms that the primary and secondary spirals in S+S pairs follow a Holmberg effect correlation on sSFR.
C1 [Cao, Chen] Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Shandong, Peoples R China.
[Cao, Chen] Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai 264209, Shandong, Peoples R China.
[Cao, Chen; Xu, Cong Kevin; Lu, Nanyao; Mazzarella, Joe] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Domingue, Donovan; Ronca, Joseph; Jacques, Allison] Georgia Coll & State Univ, CBX 82, Milledgeville, GA 31061 USA.
[Buat, Veronique] Univ Aix Marseille, LAM, 38 Rue F Joliot Curie, F-13388 Marseille 13, France.
[Buat, Veronique] CNRS, UMR7326, 38 Rue F Joliot Curie, F-13388 Marseille 13, France.
[Cheng, Yi-Wen] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
[Gao, Yu] Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China.
[Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Jarrett, Thomas H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Lisenfeld, Ute] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
[Sun, Wei-Hsin] Natl Taiwan Univ, Inst Astrophys, Taipei, Taiwan.
[Sun, Wei-Hsin] Natl Museum Nat Sci, Taipei, Taiwan.
[Wu, Hong] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China.
[Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Cao, C (reprint author), Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Shandong, Peoples R China.; Cao, C (reprint author), Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai 264209, Shandong, Peoples R China.; Cao, C; Xu, CK (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
EM caochen@sdu.edu.cn; cxu@ipac.caltech.edu
RI Lisenfeld, Ute/A-1637-2015
OI Lisenfeld, Ute/0000-0002-9471-5423
FU Spanish Ministerio de Economia y Competividad [AYA2011-24728,
AYA2014-53506-P]; Junta de Andalucia (Spain); [NSFC-11503013];
[NSFC-11420101002]; [NSFC-10978014]; [NSFC-11173059];
[NSFC-11390373]; [CAS-XDB09000000]
FX We thank the anonymous referee for helpful comments and suggestions. We
acknowledge useful discussions with Dr. Yinghe Zhao, and thank Dr. Yuyen
Chang for the help with data tables of 1M galaxies from SDSS+WISE. C.C.
and Y.G. are supported by NSFC-11503013, NSFC-11420101002,
NSFC-10978014, NSFC-11173059, NSFC-11390373, and CAS-XDB09000000. U.L.
acknowledges support by the research projects AYA2011-24728 and
AYA2014-53506-P from the Spanish Ministerio de Economia y Competividad
and the Junta de Andalucia (Spain). The Herschel spacecraft was
designed, built, tested, and launched under a contract with ESA, managed
by the Herschel/Planck Project team through an industrial consortium
under the overall responsibility of the prime contractor Thales Alenia
Space (Cannes), and including Astrium (Friedrichshafen), responsible for
the payload module and for system testing at the spacecraft level,
Thales Alenia Space (Turin), responsible for the service module, and
Astrium (Toulouse) responsible for the telescope, with an excess of a
hundred subcontractors. HCSS/HSpot/HIPE are joint developments by the
Herschel Science Ground Segment Consortium, consisting of ESA, the NASA
Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This
research has made use of the NASA/IPAC Extragalactic Database (NED),
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration.
NR 83
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U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2016
VL 222
IS 2
AR 16
DI 10.3847/0067-0049/222/2/16
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF4FW
UT WOS:000371304400002
ER
PT J
AU Wang, XG
Wiegand, T
Kraft, NJB
Swenson, NG
Davies, SJ
Hao, ZQ
Howe, R
Lin, YC
Ma, KP
Mi, XC
Su, SH
Sun, IF
Wolf, A
AF Wang, Xugao
Wiegand, Thorsten
Kraft, Nathan J. B.
Swenson, Nathan G.
Davies, Stuart J.
Hao, Zhanqing
Howe, Robert
Lin, Yiching
Ma, Keping
Mi, Xiangcheng
Su, Sheng-Hsin
Sun, I-Fang
Wolf, Amy
TI Stochastic dilution effects weaken deterministic effects of niche-based
processes in species rich forests
SO ECOLOGY
LA English
DT Article
DE coexistence theory; forest dynamics plot; functional dissimilarity;
habitat filtering; individual species-area relationship; null model;
pattern reconstruction; phylogenetic dissimilarity; point pattern
analysis; species interaction; stochastic dilution hypothesis
ID TROPICAL TREE COMMUNITIES; 2 TEMPERATE FORESTS; PHYLOGENETIC STRUCTURE;
FUNCTIONAL TRAITS; PLANT-COMMUNITIES; DIPTEROCARP FOREST; SEEDLING
MORTALITY; AMAZONIAN FOREST; POINT PATTERNS; BETA DIVERSITY
AB Recent theory predicts that stochastic dilution effects may result in species-rich communities with statistically independent species spatial distributions, even if the underlying ecological processes structuring the community are driven by deterministic niche differences. Stochastic dilution is a consequence of the stochastic geometry of biodiversity where the identities of the nearest neighbors of individuals of a given species are largely unpredictable. Under such circumstances, the outcome of deterministic species interactions may vary greatly among individuals of a given species. Consequently, nonrandom patterns in the biotic neighborhoods of species, which might be expected from coexistence or community assembly theory (e.g., individuals of a given species are neighbored by phylogenetically similar species), are weakened or do not emerge, resulting in statistical independence of species spatial distributions. We used data on phylogenetic and functional similarity of tree species in five large forest dynamics plots located across a gradient of species richness to test predictions of the stochastic dilution hypothesis. To quantify the biotic neighborhood of a focal species we used the mean phylogenetic (or functional) dissimilarity of the individuals of the focal species to all species within a local neighborhood. We then compared the biotic neighborhood of species to predictions from stochastic null models to test if a focal species was surrounded by more or less similar species than expected by chance. The proportions of focal species that showed spatial independence with respect to their biotic neighborhoods increased with total species richness. Locally dominant, high-abundance species were more likely to be surrounded by species that were statistically more similar or more dissimilar than expected by chance. Our results suggest that stochasticity may play a stronger role in shaping the spatial structure of species rich tropical forest communities than it does in species poorer forests. These findings represent an important step towards understanding the factors that govern the spatial configuration of local biotic communities. The stochastic dilution effect is a simple geometric mechanism that can explain why species' spatial distributions in species-rich communities approximate independence from their biotic neighborhood, even if deterministic niche processes are in effect.
C1 [Wang, Xugao; Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China.
[Wiegand, Thorsten] UFZ Helmholtz Ctr Environm Research UFZ, Dept Ecol Modelling, Permoserstr 15, D-04318 Leipzig, Germany.
[Wiegand, Thorsten] German Ctr Integrat Biodivers Res iDiv, Deutsch Pl 5e, D-04103 Leipzig, Germany.
[Kraft, Nathan J. B.; Swenson, Nathan G.] Univ Maryland, Dept Biol, Biol Psychol Bldg 144,Room 1210, College Pk, MD USA.
[Davies, Stuart J.] Smithsonian Inst, Ctr Trop Forest Sci, Smithsonian Inst Global Earth Observ, POB 37012, Washington, DC 20013 USA.
[Howe, Robert; Wolf, Amy] Univ Wisconsin, Dept Nat & Appl Sci, 2420 Nicolet Dr, Green Bay, WI 54311 USA.
[Lin, Yiching] Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan.
[Ma, Keping; Mi, Xiangcheng] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, 20 Nanxincun, Beijing 100093, Peoples R China.
[Su, Sheng-Hsin] Taiwan Forestry Res Inst, Taipei 10066, Taiwan.
[Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan.
RP Wang, XG (reprint author), Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China.
EM wangxg@iae.ac.cn
RI Wiegand, Thorsten/H-5877-2016; Kraft, Nathan/A-2817-2012; wang,
xugao/B-1111-2015
OI Wiegand, Thorsten/0000-0002-3721-2248; Kraft,
Nathan/0000-0001-8867-7806; wang, xugao/0000-0003-1207-8852
FU National Natural Science Foundation of China [31370444, 31570432];
Chinese Academy of Sciences [151221KYSB20130003]; ERC [233066]; United
States National Science Foundation [DEB-1046113]
FX This study was supported by the National Natural Science Foundation of
China (31370444 and 31570432), and the Chinese Academy of Sciences
(151221KYSB20130003). T. Wiegand was supported by the ERC advanced grant
233066. N. G. Swenson was supported by the United States National
Science Foundation (DEB-1046113). Data collections were founded by many
organizations, such as National Science Foundation, the Smithsonian
Tropical Research Institute, the John D. and Catherine T. MacArthur
Foundation, the Mellon Foundation, the Celera Foundation, the 1923 Fund,
and Ministry of Science and Technology in Taiwan. We also thank the
hundreds of field workers who collected data in the plots used here. T.
Paine, D. Ackerly, D. Laughlin, and three anonymous referees provided
valuable comments on earlier versions of the manuscript.
NR 60
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U1 14
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PU WILEY
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD FEB
PY 2016
VL 97
IS 2
BP 347
EP 360
DI 10.1890/14-2357.1
PG 14
WC Ecology
SC Environmental Sciences & Ecology
GA DF6BJ
UT WOS:000371439800008
PM 27145610
ER
PT J
AU Brashears, J
Aiello, A
Seymoure, BM
AF Brashears, Jake
Aiello, Annette
Seymoure, Brett M.
TI Cool Bands: Wing bands decrease rate of heating, but not equilibrium
temperature in Anartia fatima
SO JOURNAL OF THERMAL BIOLOGY
LA English
DT Article
DE Butterfly Coloration; Radiation; Reflectance; Thermoregulation
ID BEHAVIORAL THERMOREGULATION; COLIAS BUTTERFLIES; LEPIDOPTERA;
POLYMORPHISM; NYMPHALIDAE; ABSORPTION; EVOLUTION; PATTERN; COLOR
AB Butterflies regulate their internal thoracic temperature in order to optimize performance activities (e.g. flight, foraging). Previous research has shown that butterfly wings, particularly the innermost portions, play a role in thermoregulation. We investigated to see whether a lightly colored wing band would alter the thermal properties of the banded peacock butterfly (Anartia fatima) with two within subject experiments in a laboratory setting: (1) band color manipulation in which euthanized individuals were heated to thermal equilibrium with the band unaltered and then again with the wing darkened; (2) wing ablation in which individuals already run through experiment 1 were heated to equilibrium two more times; once with the outer portion of the wing including the band removed and then with the entire wing removed. Individuals were spread so that the dorsal surface of the wing was exposed to illumination from a lamp suspended above. Twelve Anartia fatima males were collected in Panama and were run through experiment one. Four individuals were run through experiment two. We found no effect of darkening the band on the internal thoracic equilibrium temperature, but the darkened band did increase the rate of heating. The wing ablation experiment revealed that wing removal lowered the internal thoracic equilibrium temperature but did not affect the heating rate. Therefore we show that butterfly bands may be important in butterfly thermoregulation and we discuss the importance of the wing band on thermoregulatory abilities in Anartia fatima with respect to the butterfly's natural history. We conclude that the wing band may allow butterflies to reduce heat stress induced by their warm environments. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Brashears, Jake] San Diego City Coll, Dept Life Sci, San Diego, CA 92101 USA.
[Aiello, Annette; Seymoure, Brett M.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Seymoure, Brett M.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
RP Seymoure, BM (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
EM jbrashea@sdccd.edu; aielloa@si.edu; brett.seymoure@asu.edu
FU Arizona State University; Smithsonian Tropical Research Institute
(STRI); School of Life Sciences Research Training Initiatives Office at
ASU
FX This work was supported by Arizona State University and the Smithsonian
Tropical Research Institute (STRI). The School of Life Sciences Research
Training Initiatives Office at ASU provided funding for the materials
required for this study. We thank Autoridad Nacional del Ambiente and
the Republic of Panamanian for the collecting permit (DAPVS-0478-2015).
We are grateful for comments and suggestions from RL Rutowski, R. De
Keyser, and an anonymous reviewer, which greatly improved this
manuscript.
NR 30
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U1 2
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0306-4565
J9 J THERM BIOL
JI J. Therm. Biol.
PD FEB
PY 2016
VL 56
BP 100
EP 108
DI 10.1016/j.jtherbio.2016.01.007
PG 9
WC Biology; Zoology
SC Life Sciences & Biomedicine - Other Topics; Zoology
GA DF2SJ
UT WOS:000371193800013
PM 26857983
ER
PT J
AU Fairen, AG
Dohm, JM
Rodriguez, JAP
Uceda, ER
Kargel, J
Soare, R
Cleaves, HJ
Oehler, D
Schulze-Makuch, D
Essefi, E
Banks, ME
Komatsu, G
Fink, W
Robbins, S
Yan, JG
Miyamoto, H
Maruyama, S
Baker, VR
AF Fairen, Alberto G.
Dohm, James M.
Rodriguez, J. Alexis P.
Uceda, Esther R.
Kargel, Jeffrey
Soare, Richard
Cleaves, H. James
Oehler, Dorothy
Schulze-Makuch, Dirk
Essefi, Elhoucine
Banks, Maria E.
Komatsu, Goro
Fink, Wolfgang
Robbins, Stuart
Yan, Jianguo
Miyamoto, Hideaki
Maruyama, Shigenori
Baker, Victor R.
TI The Argyre Region as a Prime Target for in situ Astrobiological
Exploration of Mars
SO ASTROBIOLOGY
LA English
DT Article
ID MARTIAN ATMOSPHERE; GALE CRATER; CONTINENTAL-CRUST; ISOTOPIC EVIDENCE;
NORTHERN PLAINS; ARCHEAN LIFE; WATER; EVOLUTION; OCEANS; EARTH
AB At the time before similar to 3.5 Ga that life originated and began to spread on Earth, Mars was a wetter and more geologically dynamic planet than it is today. The Argyre basin, in the southern cratered highlands of Mars, formed from a giant impact at similar to 3.93 Ga, which generated an enormous basin approximately 1800 km in diameter. The early post-impact environment of the Argyre basin possibly contained many of the ingredients that are thought to be necessary for life: abundant and long-lived liquid water, biogenic elements, and energy sources, all of which would have supported a regional environment favorable for the origin and the persistence of life. We discuss the astrobiological significance of some landscape features and terrain types in the Argyre region that are promising and accessible sites for astrobiological exploration. These include (i) deposits related to the hydrothermal activity associated with the Argyre impact event, subsequent impacts, and those associated with the migration of heated water along Argyre-induced basement structures; (ii) constructs along the floor of the basin that could mark venting of volatiles, possibly related to the development of mud volcanoes; (iii) features interpreted as ice-cored mounds (open-system pingos), whose origin and development could be the result of deeply seated groundwater upwelling to the surface; (iv) sedimentary deposits related to the formation of glaciers along the basin's margins, such as evidenced by the ridges interpreted to be eskers on the basin floor; (v) sedimentary deposits related to the formation of lakes in both the primary Argyre basin and other smaller impact-derived basins along the margin, including those in the highly degraded rim materials; and (vi) crater-wall gullies, whose morphology points to a structural origin and discharge of (wet) flows. Key Words: Mars-Surface processes and composition of Mars-Liquid water-Geological conditions for the development of life-Planetary habitability and biosignatures. Astrobiology 16, 143-158.
C1 [Fairen, Alberto G.] Ctr Astrobiol CSIC INTA, Dept Planetol & Habitabil, Madrid, Spain.
[Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Dohm, James M.; Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo, Japan.
[Rodriguez, J. Alexis P.; Banks, Maria E.] Planetary Sci Inst, Tucson, AZ USA.
[Uceda, Esther R.] Univ Autonoma Madrid, Fac Ciencias, E-28049 Madrid, Spain.
[Kargel, Jeffrey; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Soare, Richard] Dawson Coll, Dept Geog, Montreal, PQ H3Z 1A4, Canada.
[Cleaves, H. James; Maruyama, Shigenori] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 152, Japan.
[Cleaves, H. James] Inst Adv Study, Olden Lane, Princeton, NJ 08540 USA.
[Oehler, Dorothy] NASA, Lyndon B Johnson Space Ctr, Jacobs LZ Technol, JETS Contract, Houston, TX 77058 USA.
[Schulze-Makuch, Dirk] Tech Univ Berlin, Ctr Astron & Astrophys, Berlin, Germany.
[Schulze-Makuch, Dirk] Washington State Univ, Sch Environm, Pullman, WA 99164 USA.
[Essefi, Elhoucine] Univ Gabes, Higher Inst Appl Sci & Technol, Gabes, Tunisia.
[Banks, Maria E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Komatsu, Goro] Univ G dAnnunzio, Int Res Sch Planetary Sci, Pescara, Italy.
[Fink, Wolfgang] Univ Arizona, Dept Elect & Comp Engn, Coll Engn, Tucson, AZ 85721 USA.
[Fink, Wolfgang] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Robbins, Stuart] Southwest Res Inst, Boulder, CO USA.
[Yan, Jianguo] Natl Astron Observ Japan, RISE Project Off, Oshu, Japan.
RP Fairen, AG (reprint author), Ctr Astrobiol, M-108,Km 4, Madrid 28850, Spain.
EM agfairen@cab.inta-csic.es
RI Komatsu, Goro/I-7822-2012; Miyamoto, Hideaki/B-9666-2008;
OI Komatsu, Goro/0000-0003-4155-108X; Schulze-Makuch,
Dirk/0000-0002-1923-9746; Cleaves, Henderson/0000-0003-4101-0654
FU European Research Council [307496, 339231]; NASA PGG Program; JSPS
KAKENHI [26106002]; Tokyo Institute of Technology's Earth-Life Science
Institute; Astromaterials Research and Exploration Science Division at
Johnson Space Center
FX The research leading to these results is a contribution from the Project
"icyMARS,'' funded by the European Research Council, Starting Grant no
307496. J.M.D. was supported by the NASA PG&G Program and JSPS KAKENHI
Grant Number 26106002 [Hadean BioScience (Grant-in-Aid for Scientific
Research on Innovative Areas)]. J.M.D. and H.M. express their gratitude
to the Tokyo Dome Corporation for their support of the TeNQ exhibit and
the branch of Space Exploration Education & Discovery, the University
Museum, the University of Tokyo. H.J.C. would like to thank the Tokyo
Institute of Technology's Earth-Life Science Institute for funding
during the preparation of this manuscript. D.Z.O. is grateful to the
Astromaterials Research and Exploration Science Division at Johnson
Space Center for support. D.S.-M. was supported by European Research
Council, Advanced Grant "Habitability of Martian Environments,'' no
339231. The authors want to thank Chris McKay for a constructive review
of this paper.
NR 115
TC 1
Z9 1
U1 4
U2 16
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD FEB 1
PY 2016
VL 16
IS 2
BP 143
EP 158
DI 10.1089/ast.2015.1396
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DF0FB
UT WOS:000371013300003
PM 26836592
ER
PT J
AU Augspurger, CK
Franson, SE
Cushman, KC
Muller-Landau, HC
AF Augspurger, Carol K.
Franson, Susan E.
Cushman, Katherine C.
Muller-Landau, Helene C.
TI Intraspecific variation in seed dispersal of a Neotropical tree and its
relationship to fruit and tree traits
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Crown area; crown height; functional traits; recruitment; seed shadow;
tails of distribution; wind dispersal; wing loading
ID LONG-DISTANCE DISPERSAL; WIND DISPERSAL; SPATIAL-PATTERNS; TROPICAL
TREE; PLATYPODIUM-ELEGANS; TERMINAL VELOCITY; RAIN-FOREST; RECRUITMENT;
MORPHOLOGY; SEEDLINGS
AB The distribution of wind-dispersed seeds around a parent tree depends on diaspore and tree traits, as well as wind conditions and surrounding vegetation. This study of a neotropical canopy tree, Platypodium elegans, explored the extent to which parental variation in diaspore and tree traits explained (1) rate of diaspore descent in still air, (2) distributions of diaspores dispersed from a 40-m tower in the forest, and (3) natural diaspore distributions around the parent tree. The geometric mean rate of descent in still air among 20 parents was highly correlated with geometric mean wing loading(1/2) (r=0.84). However, diaspore traits and rate of descent predicted less variation in dispersal distance from the tower, although descent rate(-1) consistently correlated with dispersal distance. Measured seed shadows, particularly their distribution edges, differed significantly among six parents (DBH range 62-181cm) and were best fit by six separate anisotropic dispersal kernels and surveyed fecundities. Measured rate of descent and tree traits, combined in a mechanistic seed dispersal model, did not significantly explain variation among parents in natural seed dispersal distances, perhaps due to the limited power to detect effects with only six trees. Seedling and sapling distributions were at a greater mean distance from the parents than seed distributions; saplings were heavily concentrated at far distances. Variation among parents in the distribution tails so critical for recruitment could not be explained by measured diaspore or tree traits with this sample size, and may be determined more by wind patterns and the timing of abscission in relation to wind conditions. Studies of wind dispersal need to devote greater field efforts at recording the rare dispersal events that contribute to far dispersal distances, following their consequences, and in understanding the mechanisms that generate them.
C1 [Augspurger, Carol K.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
[Franson, Susan E.] EPA, 26 W Martin Luther King Jr Dr, Cincinnati, OH 45268 USA.
[Cushman, Katherine C.; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama.
[Cushman, Katherine C.] Brown Univ, Dept Ecol & Evolutionary Biol, 80 Waterman St, Providence, RI 02912 USA.
RP Augspurger, CK (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
EM carolaug@illinois.edu
FU NSF [BSR 8219856]
FX This research was supported by an NSF grant (BSR 8219856).
NR 46
TC 0
Z9 1
U1 14
U2 20
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD FEB
PY 2016
VL 6
IS 4
BP 1128
EP 1142
DI 10.1002/ece3.1905
PG 15
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DF1AC
UT WOS:000371069800021
PM 26839686
ER
PT J
AU Visser, MD
Bruijning, M
Wright, SJ
Muller-Landau, HC
Jongejans, E
Comita, LS
de Kroon, H
AF Visser, Marco D.
Bruijning, Marjolein
Wright, S. Joseph
Muller-Landau, Helene C.
Jongejans, Eelke
Comita, Liza S.
de Kroon, Hans
TI Functional traits as predictors of vital rates across the life cycle of
tropical trees
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE adult stature; leaf mass per area; model averaging; seed size; tree
growth; tree mortality; wood density
ID LEAF ECONOMICS SPECTRUM; MIXED-EFFECTS MODELS; RAIN-FOREST TREES;
INTERSPECIFIC VARIATION; NEOTROPICAL FORESTS; LIGHT AVAILABILITY;
DEMOGRAPHIC RATES; SPATIAL VARIATION; PRACTICAL GUIDE; PLANT ECOLOGY
AB The functional traits' of species have been heralded as promising predictors for species' demographic rates and life history. Multiple studies have linked plant species' demographic rates to commonly measured traits. However, predictive power is usually low - raising questions about the practical usefulness of traits - and analyses have been limited to size-independent univariate approaches restricted to a particular life stage. Here we directly evaluated the predictive power of multiple traits simultaneously across the entire life cycle of 136 tropical tree species from central Panama. Using a model-averaging approach, we related wood density, seed mass, leaf mass per area and adult stature (maximum diameter) to onset of reproduction, seed production, seedling establishment, and growth and survival at seedling, sapling and adult stages. Three of the four traits analysed here (wood density, seed mass and adult stature) typically explained 20-60% of interspecific variation at a given vital rate and life stage. There were strong shifts in the importance of different traits throughout the life cycle of trees, with seed mass and adult stature being most important early in life, and wood density becoming most important after establishment. Every trait had opposing effects on different vital rates or at different life stages; for example, seed mass was associated with higher seedling establishment and lower initial survival, wood density with higher survival and lower growth, and adult stature with decreased juvenile but increased adult growth and survival. Forest dynamics are driven by the combined effects of all demographic processes across the full life cycle. Application of a multitrait and full-life cycle approach revealed the full role of key traits, and illuminated how trait effects on demography change through the life cycle. The effects of traits on one life stage or vital rate were sometimes offset by opposing effects at another stage, revealing the danger of drawing broad conclusions about functional trait-demography relationships from analysis of a single life stage or vital rate. Robust ecological and evolutionary conclusions about the roles of functional traits rely on an understanding of the relationships of traits to vital rates across all life stages.
C1 [Visser, Marco D.; Bruijning, Marjolein; Jongejans, Eelke; de Kroon, Hans] Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Expt Plant Ecol & Anim Ecol, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
[Visser, Marco D.; Bruijning, Marjolein; Jongejans, Eelke; de Kroon, Hans] Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Physiol, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
[Visser, Marco D.; Wright, S. Joseph; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama.
[Comita, Liza S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
RP Visser, MD (reprint author), Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Expt Plant Ecol & Anim Ecol, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.; Visser, MD (reprint author), Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Physiol, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.; Visser, MD (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama.
EM m.visser@science.ru.nl
RI Jongejans, Eelke/B-4832-2008; de Kroon, Hans/B-3359-2009; Wright,
Stuart/M-3311-2013
OI Jongejans, Eelke/0000-0003-1148-7419; de Kroon,
Hans/0000-0001-6151-3561; Wright, Stuart/0000-0003-4260-5676
FU Netherlands Organization for Scientific Research [NWO-ALW 801-01-009];
Smithsonian Tropical Research Institute; HSBC Climate Partnership;
National Science Foundation [DEB 0425651 0948585, 1242622 1464389];
Centre for Tropical Forest Science; John D. and Catherine T. MacArthur
Foundation; Mellon Foundation; Small World Institute Fund
FX We thank Timothy Paine and an anonymous reviewer for helpful comments.
This study was supported by the Netherlands Organization for Scientific
Research (NWO-ALW 801-01-009; MDV), the Smithsonian Tropical Research
Institute (MDV, MB) and the HSBC Climate Partnership (HCM). The data
sets were collected with funding from the National Science Foundation
(DEB 0425651 & 0948585 to SPH and 1242622 & 1464389 to LSC), the
Smithsonian Tropical Research Institute, the Centre for Tropical Forest
Science, the John D. and Catherine T. MacArthur Foundation, the Mellon
Foundation and the Small World Institute Fund.
NR 69
TC 12
Z9 12
U1 17
U2 53
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0269-8463
EI 1365-2435
J9 FUNCT ECOL
JI Funct. Ecol.
PD FEB
PY 2016
VL 30
IS 2
BP 168
EP 180
DI 10.1111/1365-2435.12621
PG 13
WC Ecology
SC Environmental Sciences & Ecology
GA DE9JU
UT WOS:000370953700002
ER
PT J
AU Petter, G
Wagner, K
Wanek, W
Delgado, EJS
Zotz, G
Cabral, JS
Kreft, H
AF Petter, Gunnar
Wagner, Katrin
Wanek, Wolfgang
Delgado, Eduardo Javier Sanchez
Zotz, Gerhard
Cabral, Juliano Sarmento
Kreft, Holger
TI Functional leaf traits of vascular epiphytes: vertical trends within the
forest, intra- and interspecific trait variability, and taxonomic
signals
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE carbon isotope ratio C-13; LDMC; leaf chlorophyll concentration; leaf
thickness; leaf nitrogen concentration; leaf water content; nitrogen
isotope ratio N-15; specific leaf area (SLA); variance partitioning;
vertical zonation
ID ENVIRONMENTAL GRADIENT; ECONOMICS SPECTRUM; SPATIAL STRUCTURE; WATER
RELATIONS; TREE HEIGHT; RAIN-FOREST; DRY FOREST; NITROGEN; CARBON; LIGHT
AB Analysing functional traits along environmental gradients can improve our understanding of the mechanisms structuring plant communities. Within forests, vertical gradients in light intensity, temperature and humidity are often pronounced. Vascular epiphytes are particularly suitable for studying the influence of these vertical gradients on functional traits because they lack contact with the soil and thus individual plants are entirely exposed to different environmental conditions, from the dark and humid understorey to the sunny and dry outer canopy. In this study, we analysed multiple aspects of the trait-based ecology of vascular epiphytes: shifts in trait values with height above ground (as a proxy for vertical environmental gradients) at community and species level, the importance of intra- vs. interspecific trait variability, and trait differences among taxonomic groups. We assessed ten leaf traits for 1151 individuals belonging to 83 epiphyte species of all major taxonomic groups co-occurring in a Panamanian lowland forest. Community mean trait values of many leaf traits were strongly correlated with height and particularly specific leaf area and chlorophyll concentration showed nonlinear, negative trends. Intraspecific trait variability was pronounced and accounted for one-third of total observed trait variance. Intraspecific trait adjustments along the vertical gradient were common and seventy per cent of all species showed significant trait-height relationships. In addition, intraspecific trait variability was positively correlated with the vertical range occupied by species. We observed significant trait differences between major taxonomic groups (orchids, ferns, aroids, bromeliads). In ferns, for instance, leaf dry matter content was almost twofold higher than in the other taxonomic groups. This indicates that some leaf traits are taxonomically conserved. Our study demonstrates that vertical environmental gradients strongly influence functional traits of vascular epiphytes. In order to understand community composition along such gradients, it is central to study several aspects of trait-based ecology, including both community and intraspecific trends of multiple traits.
C1 [Petter, Gunnar; Cabral, Juliano Sarmento; Kreft, Holger] Univ Gottingen, Biodivers Macroecol & Conservat Biogeog Grp, D-37073 Gottingen, Germany.
[Wagner, Katrin; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, Funct Ecol Grp, D-26111 Oldenburg, Germany.
[Wanek, Wolfgang] Univ Vienna, Dept Microbiol & Ecosyst Sci, Vienna, Austria.
[Delgado, Eduardo Javier Sanchez; Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama.
[Delgado, Eduardo Javier Sanchez] Univ Panama, Panama City, Panama.
RP Petter, G (reprint author), Univ Gottingen, Biodivers Macroecol & Conservat Biogeog Grp, D-37073 Gottingen, Germany.
EM gpetter@uni-goettingen.de
RI Wanek, Wolfgang/E-7001-2012; Sarmento Cabral, Juliano/K-3973-2012
OI Wanek, Wolfgang/0000-0003-2178-8258; Sarmento Cabral,
Juliano/0000-0002-0116-220X
FU Deutsche Forschungsgemeinschaft (DFG) [Zo 94/5-1]; DFG Initiative of
Excellence Free Floater Program at the University of Gottingen; DFG
[SA-21331]
FX We thank the Republic of Panama for making its natural resources
available for science (research and export permits: SE/P-3-11 and
SEX/P-27-11). Thanks to all the people of the Tropical Canopy Biology
Program at STRI who made work at the crane possible. Fieldwork in Panama
by GZ, KW and ES was funded by the Deutsche Forschungsgemeinschaft (DFG;
Zo 94/5-1). GP and HK were funded by the DFG Initiative of Excellence
Free Floater Program at the University of Gottingen. JSC acknowledges
financial support by a DFG grant (SA-21331).
NR 57
TC 2
Z9 3
U1 11
U2 40
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0269-8463
EI 1365-2435
J9 FUNCT ECOL
JI Funct. Ecol.
PD FEB
PY 2016
VL 30
IS 2
BP 188
EP 198
DI 10.1111/1365-2435.12490
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA DE9JU
UT WOS:000370953700004
ER
PT J
AU Enochs, IC
Manzello, DP
Wirshing, HH
Carlton, R
Serafy, J
AF Enochs, I. C.
Manzello, D. P.
Wirshing, H. H.
Carlton, R.
Serafy, J.
TI Micro-CT analysis of the Caribbean octocoral Eunicea flexuosa subjected
to elevated pCO(2)
SO ICES JOURNAL OF MARINE SCIENCE
LA English
DT Article
DE calcification; micro-CT; ocean acidification; octocoral; sclerite
ID CRUSTOSE CORALLINE ALGAE; REGION-WIDE DECLINES; OCEAN ACIDIFICATION;
GORGONIANS COELENTERATA; CARBON-DIOXIDE; CLIMATE-CHANGE; REEF; SEAWATER;
WATER; DISSOCIATION
AB Rising anthropogenic carbon dioxide has resulted in a drop in ocean pH, a phenomenon known as ocean acidification (OA). These acidified waters have many ramifications for diverse marine biota, especially those species which precipitate calcium carbonate skeletons. The permanence of coral reef ecosystems is therefore closely related to OA stress as habitat-forming corals will exhibit reduced calcification and growth. Relatively little is known concerning the fate of other constituent taxa which may either suffer concomitant declines or be competitively favoured in acidified waters. Here, we experimentally (49 d) test the effects of next century predictions for OA (pH = 7.75, pCO(2) = 1081 mu atm) vs. near-present-day conditions (pH = 8.01, pCO(2) = 498 mu atm) on the common Caribbean octocoral Eunicea flexuosa. We measure linear extension of this octocoral and use a novel technique, high-resolution micro-computed tomography, to measure potential differences in the morphology of calcified internal skeletal structures (sclerites) in a 2 mm apical section of each branch. Despite the use of highly accurate procedures, we found no significant differences between treatments in either the growth of E. flexuosa branches or the structure of their sclerites. Our results suggest a degree of resilience to OA stress and provide evidence that this octocoral species may persist on Caribbean coral reefs, despite global change.
C1 [Enochs, I. C.; Carlton, R.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Studies, 4600 Rickenbacker Cswy, Miami, FL 33149 USA.
[Enochs, I. C.; Manzello, D. P.; Carlton, R.] NOAA, Atlantic Oceanog & Meteorol Lab, 4301 Rickenbacker Cswy, Miami, FL 33149 USA.
[Wirshing, H. H.] Natl Museum Nat Hist, Smithsonian Inst, Box 37012,MRC 163, Washington, DC 20013 USA.
[Serafy, J.] NOAA, Southeast Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA.
RP Enochs, IC (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Studies, 4600 Rickenbacker Cswy, Miami, FL 33149 USA.; Enochs, IC (reprint author), NOAA, Atlantic Oceanog & Meteorol Lab, 4301 Rickenbacker Cswy, Miami, FL 33149 USA.
EM ienochs@rsmas.miami.edu
RI Manzello, Derek/A-8661-2014; Enochs, Ian/B-8051-2014
OI Manzello, Derek/0000-0002-0720-3041; Enochs, Ian/0000-0002-8867-0361
FU NOAA's CRCP; OAP
FX We gratefully acknowledge funding from NOAA's CRCP and OAP.
NR 67
TC 2
Z9 2
U1 3
U2 12
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1054-3139
EI 1095-9289
J9 ICES J MAR SCI
JI ICES J. Mar. Sci.
PD FEB-MAR
PY 2016
VL 73
IS 3
BP 910
EP 919
DI 10.1093/icesjms/fsv159
PG 10
WC Fisheries; Marine & Freshwater Biology; Oceanography
SC Fisheries; Marine & Freshwater Biology; Oceanography
GA DF2AR
UT WOS:000371142000038
ER
PT J
AU Bluthgen, N
Simons, NK
Jung, K
Prati, D
Renner, SC
Boch, S
Fischer, M
Holzel, N
Klaus, VH
Kleinebecker, T
Tschapka, M
Weisser, WW
Gossner, MM
AF Bluethgen, Nico
Simons, Nadja K.
Jung, Kirsten
Prati, Daniel
Renner, Swen C.
Boch, Steffen
Fischer, Markus
Hoelzel, Norbert
Klaus, Valentin H.
Kleinebecker, Till
Tschapka, Marco
Weisser, Wolfgang W.
Gossner, Martin M.
TI Land use imperils plant and animal community stability through changes
in asynchrony rather than diversity
SO NATURE COMMUNICATIONS
LA English
DT Article
ID ECOSYSTEM STABILITY; STATISTICAL INEVITABILITY; GRASSLAND EXPERIMENT;
SPECIES RICHNESS; USE INTENSITY; FOOD WEBS; BIODIVERSITY; PRODUCTIVITY;
FERTILIZATION; RESILIENCE
AB Human land use may detrimentally affect biodiversity, yet long-term stability of species communities is vital for maintaining ecosystem functioning. Community stability can be achieved by higher species diversity (portfolio effect), higher asynchrony across species (insurance hypothesis) and higher abundance of populations. However, the relative importance of these stabilizing pathways and whether they interact with land use in real-world ecosystems is unknown. We monitored inter-annual fluctuations of 2,671 plant, arthropod, bird and bat species in 300 sites from three regions. Arthropods show 2.0-fold and birds 3.7-fold higher community fluctuations in grasslands than in forests, suggesting a negative impact of forest conversion. Land-use intensity in forests has a negative net impact on stability of bats and in grasslands on birds. Our findings demonstrate that asynchrony across species-much more than species diversity alone-is the main driver of variation in stability across sites and requires more attention in sustainable management.
C1 [Bluethgen, Nico] Tech Univ Darmstadt, Dept Biol, Schnittspahnstr 3, D-64287 Darmstadt, Germany.
[Simons, Nadja K.; Weisser, Wolfgang W.; Gossner, Martin M.] Tech Univ Munich, Ctr Life & Food Sci Weihenstephan, Dept Ecol & Ecosyst Management, Terr Ecol Res Grp, Hans Carl von Carlowitz Pl 2, D-85354 Freising Weihenstephan, Germany.
[Jung, Kirsten; Tschapka, Marco] Univ Ulm, Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany.
[Prati, Daniel; Boch, Steffen; Fischer, Markus] Univ Bern, Inst Plant Sci, Altenbergrain 21, CH-3013 Bern, Switzerland.
[Renner, Swen C.] Univ Nat Resources & Life Sci, Inst Zool, Gregor Mendel Str 33, A-1180 Vienna, Austria.
[Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Fischer, Markus] Senckenberg Gesell Nat Forsch Biodivers & Climate, D-60325 Frankfurt, Germany.
[Hoelzel, Norbert; Klaus, Valentin H.; Kleinebecker, Till] Univ Munster, Inst Landscape Ecol, Heisenbergstr 2, D-48149 Munster, Germany.
RP Bluthgen, N (reprint author), Tech Univ Darmstadt, Dept Biol, Schnittspahnstr 3, D-64287 Darmstadt, Germany.
EM bluethgen@bio.tu-darmstadt.de
RI Fischer, Markus/C-6411-2008; Bluthgen, Nico/F-5983-2010; Boch,
Steffen/L-5436-2016; Fachbereich14, Dekanat/C-8553-2015; Gossner, Martin
M./J-2730-2015; Holzel, Norbert/H-8753-2013;
OI Fischer, Markus/0000-0002-5589-5900; Gossner, Martin
M./0000-0003-1516-6364; Renner, Swen/0000-0002-6893-4219
FU DFG [1374]
FX Yann Hautier and Kevin Gross provided helpful comments on an earlier
draft. We thank Stefan Bohm (birds and bats), Barbara Schmitt, Stefan
Blaser, Stephanie Socher, Jorg Muller, Judith Minker, Thorsten Meene and
Ulf Pommer (plants), Esther Pasalic, Markus Lange, Manfred Turke, Iris
Gallenberger, Steffen Both, Norbert Leber, Kaspar Kremer, Ellen Sperr,
Luis Sikora, Marco Lutz and Petra Freynhagen (arthropods) for collecting
data in the field, Boris Buche, Roland Achtziger, Thomas Wagner, Torben
Kolckebeck, Frank Kohler, Theo Blick, Franz Schmolke, Michael-Andreas
Fritze, Gunter Kohler, Anne Kastner and Oliver Wiche for arthropod
species identification. We thank the managers of the three
Exploratories, Katrin Hartwich, Sonja Gockel, Kerstin Wiesner, and
Martin Gorke for their work in maintaining the plot and project
infrastructure; Christiane Fischer and Simone Pfeiffer for giving
support through the central office, Michael Owonibi for managing the
central data base; and Eduard Linsenmair, Dominik Hessenmoller, Jens
Nieschulze, Ingo Schoning, Franc,ois Buscot, Ernst-Detlef Schulze and
the late Elisabeth Kalko for their role in setting up the Biodiversity
Exploratories project. E. Kalko is also memorized for her invaluable
inspiration and for launching the studies on bats and birds. The work
has been funded by the DFG Priority Program 1374
'Infrastructure-Biodiversity-Exploratories'. Field work permits were
issued by the responsible state environmental offices of
Baden-Wurttemberg, Thuringen and Brandenburg (according to 72
BbgNatSchG). Ulrich Kern kindly allowed us to use his drawings of a
bird, beetle and true bug.
NR 52
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD FEB
PY 2016
VL 7
AR 10697
DI 10.1038/ncomms10697
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF0LA
UT WOS:000371029300002
PM 26869180
ER
PT J
AU Kennedy, JP
Pil, MW
Proffitt, CE
Boeger, WA
Stanford, AM
Devlin, DJ
AF Kennedy, John Paul
Pil, Maria W.
Proffitt, C. Edward
Boeger, Walter A.
Stanford, Alice M.
Devlin, Donna J.
TI Postglacial expansion pathways of red mangrove, Rhizophora mangle, in
the Caribbean Basin and Florida
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Caribbean; competitive exclusion; Florida; genetic diversity;
hydrochory; microsatellite; ocean current dispersal; postglacial
expansion; red mangrove; Rhizophora mangle; Rhizophoraceae
ID SPATIAL GENETIC-STRUCTURE; MULTILOCUS GENOTYPE DATA;
POPULATION-STRUCTURE; MICROSATELLITE LOCI; MIGRATION RATES; COMPARATIVE
PHYLOGEOGRAPHY; PHYLOGENETIC TREES; FINITE POPULATION; TROPICAL
ATLANTIC; MITOCHONDRIAL-DNA
AB PREMISE OF THE STUDY: The Last Glacial Maximum (LGM) was a period of massive range contraction. Post-LGM, water -dispersed coastal species, including the red mangrove (Rhizophora mangle), expanded poleward as propagules were transported by ocean currents. We assessed postglacial marine expansion pathways for R. mangle within the Caribbean Basin and Florida.
METHODS: Six microsatellite loci were used to genotype 237 individuals from nine R. mangle populations in the Caribbean, Florida, and Northwest Africa. We evaluated genetic variation, population structure, gene flow along alternative post-LGM expansion pathways to Florida, and potential long-distance dispersal (LDD) from West Africa to Caribbean islands.
KEY RESULTS: These R. mangle populations had substantial genetic structure (FsT = 0.37, P < 0.0001) with three discrete population clusters (Caribbean mainland, Caribbean islands, and Florida). Genetic connectivity along the mainland pathway (Caribbean mainland to Florida) vs. limited gene dispersal along the Antilles Island pathway (Caribbean islands to Florida) supported Florida recolonization from Caribbean mainland sources. Genetic similarity of Northwest Africa and two Caribbean islands provided evidence for trans -Atlantic LDD. We did not find a pattern of decreasing genetic diversity with latitude.
CONCLUSIONS: We outline a complex expansion history for R. mangle, with discrete pathways of recolonization for Florida and Caribbean islands. Contrary to expectation, connectivity to putative Caribbean mainland refugial populations via ocean currents, and not latitude, appears to dictate genetic diversity within Caribbean island and Florida R. mangle. These findings provide a framework for further investigation of additional water -dispersed neotropical species, and insights for management initiatives.
C1 [Kennedy, John Paul; Proffitt, C. Edward; Devlin, Donna J.] Florida Atlantic Univ, Dept Biol Sci, Harbor Branch Oceanog Inst, Ft Pierce, FL 34946 USA.
[Pil, Maria W.] Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA.
[Boeger, Walter A.] Univ Fed Parana, Dept Zool, BR-81531990 Curitiba, Parana, Brazil.
[Stanford, Alice M.] Univ Virgin Isl, Dept Biol Sci, St Thomas, VI 00802 USA.
[Kennedy, John Paul] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
RP Kennedy, JP (reprint author), Florida Atlantic Univ, Dept Biol Sci, Harbor Branch Oceanog Inst, Ft Pierce, FL 34946 USA.; Kennedy, JP (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM ennedyjp@si.edu
OI Kennedy, John Paul/0000-0002-1015-1246
FU NSF VI-EPSCoR [0814417]; Florida Atlantic University; Christensen Fund
Scholarship in Plant Conservation from the Whitney R. Harris World
Ecology Center
FX The authors thank C. Hughes, R. Shatters, A. Dickey; G. O'Corry-Crowe,
R. Ricklefs, and N. Smith for comments and suggestions that greatly
improved this work, H. Nance for laboratory supplies, L. Herren and I.
Chollett for map creation, and R. Brust, A. Chamberlain, A. Dieppa, I.
Feller, T. Frankovich, S. Jones, C. Landry, A. Pariselle, J. Raffray, R.
Runnels, and M. Warren for help with sample collections. They also thank
the Associate Editor and three anonymous reviewers for helpful comments
on earlier versions of this paper. Special thanks to A. Jara Cavieres
for laboratory assistance and unconditional support. This research was
funded by NSF VI-EPSCoR (grant 0814417 to A.M.S., D.J.D., and C.E.P.),
the Florida Atlantic University President's Challenge scholarship to
J.P.K., the Christensen Fund Scholarship in Plant Conservation from the
Whitney R. Harris World Ecology Center to M.W.P., and a generous
donation from Carolyn Stutt of the Mangrove Garden Foundation.
NR 120
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PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
EI 1537-2197
J9 AM J BOT
JI Am. J. Bot.
PD FEB
PY 2016
VL 103
IS 2
BP 260
EP 276
DI 10.3732/ajb.1500183
PG 17
WC Plant Sciences
SC Plant Sciences
GA DE5CS
UT WOS:000370649200009
PM 26838364
ER
PT J
AU Bethermin, M
De Breuck, C
Gullberg, B
Aravena, M
Bothwell, MS
Chapman, SC
Gonzalez, AH
Greve, TR
Litke, K
Ma, J
Malkan, M
Marrone, DP
Murphy, EJ
Spilker, JS
Stark, AA
Strandet, M
Vieira, JD
Weiss, A
Welikala, N
AF Bethermin, M.
De Breuck, C.
Gullberg, B.
Aravena, M.
Bothwell, M. S.
Chapman, S. C.
Gonzalez, A. H.
Greve, T. R.
Litke, K.
Ma, J.
Malkan, M.
Marrone, D. P.
Murphy, E. J.
Spilker, J. S.
Stark, A. A.
Strandet, M.
Vieira, J. D.
Weiss, A.
Welikala, N.
TI An ALMA view of the interstellar medium of the z=4.77 lensed starburst
SPT-S J213242-5802.9
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: starburst; galaxies: ISM; galaxies: high-redshift; galaxies:
star formation; submillimeter: galaxies
ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; C II EMISSION; APM
08279+5255; SUBMILLIMETER GALAXIES; DUST EMISSION; ENERGY-DISTRIBUTIONS;
PHYSICAL-PROPERTIES; MOLECULAR GAS; EVOLUTION
AB We present ALMA detections of the [NII] 205 mu m and CO(12-11) emission lines, and the tentative detection of [CI] P-3(1)-P-3(0) for the strongly lensed (mu = 5.7 +/- 0.5) dusty, star-forming galaxy SPT-S J213242-5802.9 (hereafter SPT2132-58) at z = 4.77. The [NII] and CO(12-11) lines are detected at 11.5 and 8.5 sigma levels, respectively, by our band 6 observations. The [CI] line is detected at 3.2 sigma after a reanalysis of existing band 3 data. The [CI] luminosity implies a gas mass of (3.8 +/- 1.2) x 10(10) M-circle dot, and, consequently, a very short depletion timescale of 34 +/- 13 Myr and a CO luminosity to gas mass conversion factor alpha(CO) of 1.0 +/- 0.3 M-circle dot (K km s(-1) pc(2))(-1). SPT2132-58 is an extreme starburst with an intrinsic star formation rate of 1100 +/- 200 M-circle dot/yr. We find a [CII]/[NII] ratio of 26 +/- 6, which is the highest ratio reported at z > 4. This suggests that SPT2132-58 hosts an evolved interstellar medium (0.5 Z(circle dot) < Z < 1.5 Z(circle dot)), which may be dominated by photodissociation regions. The CO(2-1) and CO(5-4) transitions have lower CO to far-infrared ratios than local and high-redshift samples, while CO(12-11) is similar to these samples, suggesting the presence of an additional very excited component or an active galactic nucleus.
C1 [Bethermin, M.; De Breuck, C.; Gullberg, B.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito 441, Santiago, Chile.
[Bothwell, M. S.] Univ Cambridge, Cavendish Lab, JJ Thompson Ave, Cambridge CB3 0HA, England.
[Chapman, S. C.] Dalhousie Univ, Halifax, NS, Canada.
[Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Litke, K.; Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, MC 220-6, Pasadena, CA 91125 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Vieira, J. D.] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, 1002 West Green St, Urbana, IL 61801 USA.
[Welikala, N.] Univ Oxford, Dept Physiscs, Denis Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
RP Bethermin, M (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM mbetherm@eso.org
OI Bethermin, Matthieu/0000-0002-3915-2015; De Breuck,
Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996
FU National Science Foundation [PLR- 1248097]; Kavli Foundation; Gordon and
Betty Moore Foundation [GBMF 947]; US National Science Foundation
[AST-1312950]; [PHY-1125897]
FX We thanks Roberto Decarli for his very useful suggestions, especially
about the choices of axes for Fig. 4, and the anonymous referee for
her/his very constructive comments. This paper makes use of the
following ALMA data: ADS/JAO. ALMA#2011.0.00957.S and
ADS/JAO.ALMA#2012.1.00994.S. ALMA is a partnership of ESO (representing
its member states), NSF (USA) and NINS (Japan), together with NRC
(Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. The SPT is
supported by the National Science Foundation through grant PLR- 1248097,
with partial support through PHY-1125897, the Kavli Foundation and the
Gordon and Betty Moore Foundation grant GBMF 947. J.D.V., K.C.L.,
D.P.M., and J.S.S. acknowledge support from the US National Science
Foundation under grant No. AST-1312950.
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR L7
DI 10.1051/0004-6361/201527739
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900010
ER
PT J
AU Ginsburg, A
Henkel, C
Ao, YP
Riquelme, D
Mann, JKF
Pillai, T
Mills, EAC
Requena-Torres, MA
Immer, K
Testi, L
Ott, J
Bally, J
Battersby, C
Darling, J
Aalto, S
Stanke, T
Kendrew, S
Kruijssen, JMD
Longmore, S
Dale, J
Guesten, R
Menten, KM
AF Ginsburg, Adam
Henkel, Christian
Ao, Yiping
Riquelme, Denise
Mann, Jens Kau Ff
Pillai, Thushara
Mills, Elisabeth A. C.
Requena-Torres, Miguel A.
Immer, Katharina
Testi, Leonardo
Ott, Juergen
Bally, John
Battersby, Cara
Darling, Jeremy
Aalto, Susanne
Stanke, Thomas
Kendrew, Sarah
Kruijssen, J. M. Diederik
Longmore, Steven
Dale, James
Guesten, Rolf
Menten, Karl M.
TI Dense gas in the Galactic central molecular zone is warm and heated by
turbulence
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Galaxy: center; ISM: molecules; ISM: structure; Galaxy: nucleus; cosmic
rays; ISM: clouds
ID STAR-FORMATION RATE; CENTER CLOUD G0.253+0.016; SGR A-ASTERISK;
INFRARED-DARK CLOUDS; MILKY-WAY; INTERSTELLAR-MEDIUM; ASTROPHYSICAL
MEDIA; PHYSICAL-PROPERTIES; SAGITTARIUS B2; CENTER REGION
AB Context. The Galactic center is the closest region where we can study star formation under extreme physical conditions like those in high-redshift galaxies.
Aims. We measure the temperature of the dense gas in the central molecular zone (CMZ) and examine what drives it.
Methods. We mapped the inner 300 pc of the CMZ in the temperature-sensitive J = 3-2 para-formaldehyde (p-H2CO) transitions. We used the 3(2,1)-2(2,0)/3(0,3)-2(0,2) line ratio to determine the gas temperature in n similar to 10(4) - 10(5) cm(-3) gas. We have produced temperature maps and cubes with 30 0 0 and 1 km s(-1) resolution and published all data in FITS form.
Results. Dense gas temperatures in the Galactic center range from similar to 60 K to > 100 K in selected regions. The highest gas temperatures T-G > 100 K are observed around the Sgr B2 cores, in the extended Sgr B2 cloud, the 20 km s(-1) and 50 km s(-1) clouds, and in "The Brick" (G0.253 + 0.016). We infer an upper limit on the cosmic ray ionization rate zeta(CR) < 10(-14) s(-1).
Conclusions. The dense molecular gas temperature of the region around our Galactic center is similar to values found in the central regions of other galaxies, in particular starburst systems. The gas temperature is uniformly higher than the dust temperature, confirming that dust is a coolant in the dense gas. Turbulent heating can readily explain the observed temperatures given the observed line widths. Cosmic rays cannot explain the observed variation in gas temperatures, so CMZ dense gas temperatures are not dominated by cosmic ray heating. The gas temperatures previously observed to be high in the inner similar to 75 pc are confirmed to be high in the entire CMZ.
C1 [Ginsburg, Adam; Immer, Katharina; Testi, Leonardo; Stanke, Thomas] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Henkel, Christian; Riquelme, Denise; Mann, Jens Kau Ff; Pillai, Thushara; Requena-Torres, Miguel A.; Guesten, Rolf; Menten, Karl M.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
[Henkel, Christian] King Abdulaziz Univ, Dept Astron, POB 80203, Jeddah 21589, Saudi Arabia.
[Ao, Yiping] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Ao, Yiping] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China.
[Mills, Elisabeth A. C.; Ott, Juergen] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Bally, John; Darling, Jeremy] Univ Colorado, CASA, 389 UCB, Boulder, CO 80309 USA.
[Battersby, Cara] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Aalto, Susanne] Chalmers, Dept Earth & Space Sci, S-41258 Gothenburg, Sweden.
[Kendrew, Sarah] Univ Oxford, Dept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Kruijssen, J. M. Diederik] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
[Longmore, Steven] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
[Dale, James] Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany.
RP Ginsburg, A (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM Adam.Ginsburg@eso.org
OI Darling, Jeremy/0000-0003-2511-2060; Kendrew, Sarah/0000-0002-7612-0469
FU Deutsche Forschungsgemeinschaft (DFG) via the SPP (priority program)
1573 "Physics of the ISM"; DFG cluster of excellence "Origin and
Structure of the Universe" (JED)
FX We thank the staff and observers at APEX for carrying out the
service-mode observations. We are grateful to Arnaud Belloche, Axel
Weiss, and Carlos de Breuck for assistance in developing the observing
strategy, and Per Bergman for his assistance in understanding the SHFI-1
baseline issues. We thank Katharine Johnston for providing the SMA
p-H2CO 32,1-22,0 data cube for The
Brick. We thank Erik Rosolowsky for advice concerning treatment of the
biases inherent in clump extraction, Padelis Papadopoulos for providing
commentary on a draft of the paper, Neale Gibson for discussions about
parameter constraints, and the referee for a helpful review. T.P.
acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) via
the SPP (priority program) 1573 "Physics of the ISM". This research was
supported by the DFG cluster of excellence "Origin and Structure of the
Universe" (JED).
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A50
DI 10.1051/0004-6361/201526100
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900061
ER
PT J
AU Hansen, TT
Andersen, J
Nordstrom, B
Beers, TC
Placco, VM
Yoon, J
Buchhave, LA
AF Hansen, T. T.
Andersen, J.
Nordstrom, B.
Beers, T. C.
Placco, V. M.
Yoon, J.
Buchhave, L. A.
TI The role of binaries in the enrichment of the early Galactic halo II.
Carbon-enhanced metal-poor stars: CEMP-no stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Galaxy: formation; Galaxy: halo; stars: chemically peculiar; binaries:
spectroscopic; ISM: structure
ID LESS-THAN -5.0; MILKY-WAY; CHEMICAL-COMPOSITION; 1ST STARS;
SPECTROSCOPIC ANALYSIS; ABUNDANCE ANALYSIS; HIGH-RESOLUTION; FE/H
LESS-THAN-OR-EQUAL-TO-3.5; SMSS J031300.36-670839.3; ATMOSPHERIC
PARAMETERS
AB Context. The detailed composition of most metal-poor halo stars has been found to be very uniform. However, a fraction of 20-70% (increasing with decreasing metallicity) exhibit dramatic enhancements in their abundances of carbon; these are the so-called carbon-enhanced metal-poor (CEMP) stars. A key question for Galactic chemical evolution models is whether this non-standard composition reflects that of the stellar natal clouds or is due to local, post-birth mass transfer of chemically processed material from a binary companion; CEMP stars should then all be members of binary systems.
Aims. Our aim is to determine the frequency and orbital parameters of binaries among CEMP stars with and without over-abundances of neutron-capture elements - CEMP-s and CEMP-no stars, respectively -as a test of this local mass-transfer scenario. This paper discusses a sample of 24 CEMP-no stars, while a subsequent paper will consider a similar sample of CEMP-s stars.
Methods. High-resolution, low S/N spectra of the stars were obtained at roughly monthly intervals over a time span of up to eight years with the FIES spectrograph at the Nordic Optical Telescope. Radial velocities of similar to 100 m s(-1) precision were determined by cross-correlation after each observing night, allowing immediate, systematic follow-up of any variable object.
Results. Most programme stars exhibit no statistically significant radial-velocity variation over this period and appear to be single, while four are found to be binaries with orbital periods of 300-2000 days and normal eccentricity; the binary frequency for the sample is 17 +/- 9%. The single stars mostly belong to the recently identified low-C band, while the binaries have higher absolute carbon abundances.
Conclusions. We conclude that the nucleosynthetic process responsible for the strong carbon excess in these ancient stars is unrelated to their binary status; the carbon was imprinted on their natal molecular clouds in the early Galactic interstellar medium (ISM) by an even earlier external source, strongly indicating that the CEMP-no stars are likely bona fide second-generation stars. We discuss potential production sites for carbon and its transfer across interstellar distances in the early ISM, and the implications for the composition of high-redshift DLA systems.
C1 [Hansen, T. T.] Heidelberg Univ, Landessternwarte, ZAH, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Andersen, J.; Nordstrom, B.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Andersen, J.; Nordstrom, B.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Beers, T. C.; Placco, V. M.; Yoon, J.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Beers, T. C.; Placco, V. M.; Yoon, J.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA.
[Buchhave, L. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
RP Hansen, TT (reprint author), Heidelberg Univ, Landessternwarte, ZAH, Konigstuhl 12, D-69117 Heidelberg, Germany.
EM thansen@lsw.uni-heidelberg.de
OI Hansen, Terese/0000-0001-6154-8983
FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881];
Danish Natural Science Research Council; Carlsberg Foundation; Physics
Frontier Center/Joint Institute or Nuclear Astrophysics (JINA); Physics
Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE)
- US National Science Foundation; [PHY 08-22648]; [PHY 14-30152]
FX We thank several NOT staff members and students for obtaining most of
the FIES observations for us in service mode during this large project.
We thank Piercarlo Bonifacio and Monique Spite for sharing their
previously obtained spectrum of CS 29527-015 and for obtaining a new
upper limit on the [Ba/Fe] ratio for this star, George Preston for very
kindly sharing his own observations of CS 22957-027, and Norbert
Christlieb for sharing his RV data for HE 0107-5240 with us. We also
thank Heather Jacobsen for advice on the best available historical RV
data for CD-24 degrees 17504, and David Yong for helping to clarify some
of the mystery regarding HE 1506-0113. Furthermore, we express our
cordial thanks to the referee for an incisive and helpful report, which
led to substantial improvements in the paper. T.T.H. was supported
during this work by Sonderforschungsbereich SFB 881 "The Milky Way
System" (subproject A4) of the German Research Foundation (DFG). J.A.
and B.N. gratefully acknowledge financial support from the Danish
Natural Science Research Council and the Carlsberg Foundation, and
T.C.B., V.M.P., and J.Y. acknowledge partial support for this work from
grants PHY 08-22648; Physics Frontier Center/Joint Institute or Nuclear
Astrophysics (JINA), and PHY 14-30152; Physics Frontier Center/JINA
Center for the Evolution of the Elements (JINA-CEE), awarded by the US
National Science Foundation. This paper is based primarily on
observations made with the Nordic Optical Telescope, operated by the
Nordic Optical Telescope Scientific Association at the Observatorio del
Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica
de Canarias. It is also based on observations obtained at the Southern
Astrophysical Research (SOAR) telescope, which is a joint project of the
Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica
Federativa do Brasil, the US National Optical Astronomy Observatory
(NOAO), the University of North Carolina at Chapel Hill (UNC), and
Michigan State University (MSU).
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A160
DI 10.1051/0004-6361/201527235
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900170
ER
PT J
AU Hogerheijde, MR
Bekkers, D
Pinilla, P
Salinas, VN
Kama, M
Andrews, SM
Qi, CH
Wilner, DJ
AF Hogerheijde, Michiel R.
Bekkers, David
Pinilla, Paola
Salinas, Vachail N.
Kama, Mihkel
Andrews, Sean M.
Qi, Chunhua
Wilner, David J.
TI Steepening of the 820 mu m continuum surface brightness profile signals
dust evolution in TW Hydrae's disk
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion; accretion disks; protoplanetary disks; circumstellar matter;
submillimeter: planetary systems dust, extinction
ID PLANET-FORMING REGION; ORION NEBULA CLUSTER; PROTOPLANETARY DISKS; TAURI
STARS; CIRCUMSTELLAR DISKS; HL TAU; SUBMILLIMETER ARRAY; TRANSITION
DISK; SOLAR NEBULA; GRAIN-GROWTH
AB Context. Grain growth in planet-forming disks is the first step toward the formation of planets. The growth of grains and their inward drift leaves a distinct imprint on the dust surface density distribution and the resulting surface brightness profile of the thermal continuum emission.
Aims. We determine the surface brightness profile of the continuum emission using resolved observations at millimeter wavelengths of the disk around TW Hya, and infer the signature of dust evolution on the surface density and dust opacity.
Methods. Archival ALMA observations at 820 mu m on baselines up to 410 k lambda are compared to parameterized disk models to determine the surface brightness profile.
Results. Under the assumption of a constant dust opacity, a broken radial power law best describes the dust surface density with a slope of 0 : 53 +/- 0 : 01 from the 4.1 au radius of the already known inner hole to a turn-over radius of 47 : 1 +/- 0 : 2 au, steepening to 8 : 0 +/- 0 : 1 at larger radii. The emission drops below the detection limit beyond similar to 60 au.
Conclusions. The shape of the dust surface density is consistent with theoretical expectations for grain growth, fragmentation, and drift, but its total dust content and its turn-over radius are too large for TW Hya's age of 8-10 Myr even when taking into account a radially varying dust opacity. Higher resolution imaging with ALMA of TW Hya and other disks is required to establish whether unseen gaps associated with, e. g., embedded planets trap grains at large radii or whether locally enhanced grain growth associated with the CO snow line explains the extent of the millimeter continuum surface brightness profile. In the latter case, population studies should reveal a correlation between the location of the CO snow line and the extent of the millimeter continuum. In the former case, and if CO freeze-out promotes planet formation, this correlation should extend to the location of gaps as well.
C1 [Hogerheijde, Michiel R.; Bekkers, David; Pinilla, Paola; Salinas, Vachail N.; Kama, Mihkel] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Andrews, Sean M.; Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS42, Cambridge, MA 02138 USA.
RP Hogerheijde, MR (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM michiel@strw.leidenuniv.nl
FU Netherlands Organization for Scientific Research (NWO); Netherlands
Research School for Astronomy (NOVA)
FX This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2011.0.00340.S and ADS/JAO.ALMA#2011.0.00399.S. ALMA is a
partnership of ESO (representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The
research of M.R.H. and V.N.S. is supported by grants from the
Netherlands Organization for Scientific Research (NWO) and the
Netherlands Research School for Astronomy (NOVA). This work made use of
PyAstronomy.
NR 58
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A99
DI 10.1051/0004-6361/201527754
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900110
ER
PT J
AU Jorissen, A
Hansen, T
Van Eck, S
Andersen, J
Nordstrom, B
Siess, L
Torres, G
Masseron, T
Van Winckel, H
AF Jorissen, A.
Hansen, T.
Van Eck, S.
Andersen, J.
Nordstrom, B.
Siess, L.
Torres, G.
Masseron, T.
Van Winckel, H.
TI HE 0017+0055: A probable pulsating CEMP-rs star and long-period binary
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: carbon; stars: evolution; stars: individual: HE 0017+0055;
Galaxy: halo
ID METAL-POOR STARS; NEAR-INFRARED SPECTROSCOPY; LARGE-MAGELLANIC-CLOUD;
CARBON-RICH STARS; HORIZONTAL-BRANCH; GIANT BRANCH; CH/CN-STRONG; AGB
STARS; RED GIANT; MILKY-WAY
AB Context. A large fraction of the carbon-enhanced, extremely metal-poor halo giants ([Fe/H] < -2.5) are also strongly enriched in neutron-capture elements from the s process (CEMP-s stars). The conventional explanation for the properties of these stars is mass transfer from a nearby binary companion on the asymptotic giant branch (AGB). This scenario leads to a number of testable predictions in terms of the properties of the putative binary system and the resulting abundance pattern. Among the CEMP stars, some stars further exhibit overabundances in r-process elements on top of the s-process enrichment, and are tagged CEMP-rs stars. Although the nucleosynthesis process responsible for this kind of mixed abundance pattern is still under debate, CEMP-rs stars seem to belong to binary systems as do CEMP-s stars.
Aims. Our aim is to present and analyse in detail our comprehensive data set of systematic radial-velocity measurements and highresolution spectroscopy of the CEMP star HE 0017+0055.
Methods. Our precise radial-velocity monitoring of HE 0017+0055 over 2940 days (8 yr) with the Nordic Optical Telescope and Mercator telescopes exhibits variability, with a period of 384 d and amplitude of 540 +/- 27 m s(-1) superimposed on a nearly linear long-term decline of similar to 1 m s(-1) day(-1). We used high-resolution HERMES/Mercator and Keck/HIRES spectra to derive elemental abundances with 1D LTE MARCS models. A metallicity of [Fe/H] similar to -2.4 is found, along with s-process overabundances of the order of 2 dex (with the exception of [Y/Fe] similar to +0.5), and most notably overabundances of r-process elements like Sm, Eu, Dy, and Er in the range 0.9-2.0 dex. With [Ba/Fe] > 1.9 dex and [Eu/Fe] = 2.3 dex, HE 0017+0055 is a CEMP-rs star. We used the derived atmospheric parameters and abundances to infer HE 0017+0055 evolutionary status from a comparison with evolutionary tracks.
Results. HE 0017+0055 appears to be a giant star below the tip of the red giant branch. The s-process pollution must therefore originate from mass transfer from a companion formerly on the AGB, which is now a carbon-oxygen white dwarf (WD). If the 384 d velocity variations are attributed to theWD companion, its orbit must be seen almost face-on, with i similar to 2.3 degrees, because the mass function is very small: f (M-1, M-2) = (6.1 +/- 1.1)x10(-6) M-circle dot. Alternatively, theWD orbital motion could be responsible for the long-term velocity variations, with a period of several decades. The 384 d variations should then be attributed either to a low-mass inner companion (perhaps a brown dwarf, depending on the orbital inclination), or to stellar pulsations. The latter possibility is made likely by the fact that similar low-amplitude velocity variations, with periods close to 1 yr, have been reported for other CEMP stars in a companion paper. A definite conclusion about the origin of the 384 d velocity variations should however await the detection of synchronous low-amplitude photometric variations.
C1 [Jorissen, A.; Van Eck, S.; Siess, L.] Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium.
[Hansen, T.] Heidelberg Univ, Landessternwarte, ZAH, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Andersen, J.; Nordstrom, B.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Andersen, J.; Nordstrom, B.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Torres, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Masseron, T.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200d,Bus 2412, B-3001 Heverlee, Belgium.
RP Jorissen, A (reprint author), Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium.; Hansen, T (reprint author), Heidelberg Univ, Landessternwarte, ZAH, Konigstuhl 12, D-69117 Heidelberg, Germany.; Andersen, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.; Andersen, J (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
EM ajorisse@ulb.ac.be; thansen@lsw.uni-heidelberg.de; ja@astro.ku.dk
FU Belgian Science Policy Office [BR/143/A2/STARLAB]; German Research
Foundation (DFG) [Sonderforschungsbereich SFB 881]; Danish Natural
Science Research Council; Carlsberg Foundation
FX This research has been funded by the Belgian Science Policy Office under
contract BR/143/A2/STARLAB. S.v.E. and L.S. are FNRS research
associates. The work of T.T.H. was supported by Sonderforschungsbereich
SFB 881 "The Milky Way System" (subproject A4) of the German Research
Foundation (DFG). J.A. and B.N. gratefully acknowledge financial support
from the Danish Natural Science Research Council and the Carlsberg
Foundation. Based on observations obtained with the HERMES spectrograph,
supported by the Fund for Scientific Research of Flanders (FWO), the
Research Council of K.U. Leuven, the Fonds National de la Recherche
Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium,
the Observatoire de Geneve, Switzerland, and the Thuringer
Landessternwarte Tautenburg, Germany.
NR 62
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PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A159
DI 10.1051/0004-6361/201526993
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900169
ER
PT J
AU Pilia, M
Hessels, JWT
Stappers, BW
Kondratiev, VI
Kramer, M
van Leeuwen, J
Weltevrede, P
Lyne, AG
Zagkouris, K
Hassall, TE
Bilous, AV
Breton, RP
Falcke, H
Griessmeier, JM
Keane, E
Karastergiou, A
Kuniyoshi, M
Noutsos, A
Oslowski, S
Serylak, M
Sobey, C
ter Veen, S
Alexov, A
Anderson, J
Asgekar, A
Avruch, IM
Bell, ME
Bentum, MJ
Bernardi, G
Birzan, L
Bonafede, A
Breitling, F
Broderick, JW
Bruggen, M
Ciardi, B
Corbel, S
de Geus, E
de Jong, A
Deller, A
Duscha, S
Eisloffel, J
Fallows, RA
Fender, R
Ferrari, C
Frieswijk, W
Garrett, MA
Gunst, AW
Hamaker, JP
Heald, G
Horneffer, A
Jonker, P
Juette, E
Kuper, G
Maat, P
Mann, G
Markoff, S
McFadden, R
McKay-Bukowski, D
Miller-Jones, JCA
Nelles, A
Paas, H
Pandey-Pommier, M
Pietka, M
Pizzo, R
Polatidis, AG
Reich, W
Rottgering, H
Rowlinson, A
Schwarz, D
Smirnov, O
Steinmetz, M
Stewart, A
Swinbank, JD
Tagger, M
Tang, Y
Tasse, C
Thoudam, S
Toribio, MC
van der Horst, AJ
Vermeulen, R
Vocks, C
van Weeren, RJ
Wijers, RAMJ
Wijnands, R
Wijnholds, SJ
Wucknitz, O
Zarka, P
AF Pilia, M.
Hessels, J. W. T.
Stappers, B. W.
Kondratiev, V. I.
Kramer, M.
van Leeuwen, J.
Weltevrede, P.
Lyne, A. G.
Zagkouris, K.
Hassall, T. E.
Bilous, A. V.
Breton, R. P.
Falcke, H.
Griessmeier, J. -M.
Keane, E.
Karastergiou, A.
Kuniyoshi, M.
Noutsos, A.
Oslowski, S.
Serylak, M.
Sobey, C.
ter Veen, S.
Alexov, A.
Anderson, J.
Asgekar, A.
Avruch, I. M.
Bell, M. E.
Bentum, M. J.
Bernardi, G.
Birzan, L.
Bonafede, A.
Breitling, F.
Broderick, J. W.
Brueggen, M.
Ciardi, B.
Corbel, S.
de Geus, E.
de Jong, A.
Deller, A.
Duscha, S.
Eisloeffel, J.
Fallows, R. A.
Fender, R.
Ferrari, C.
Frieswijk, W.
Garrett, M. A.
Gunst, A. W.
Hamaker, J. P.
Heald, G.
Horneffer, A.
Jonker, P.
Juette, E.
Kuper, G.
Maat, P.
Mann, G.
Markoff, S.
McFadden, R.
McKay-Bukowski, D.
Miller-Jones, J. C. A.
Nelles, A.
Paas, H.
Pandey-Pommier, M.
Pietka, M.
Pizzo, R.
Polatidis, A. G.
Reich, W.
Roettgering, H.
Rowlinson, A.
Schwarz, D.
Smirnov, O.
Steinmetz, M.
Stewart, A.
Swinbank, J. D.
Tagger, M.
Tang, Y.
Tasse, C.
Thoudam, S.
Toribio, M. C.
van der Horst, A. J.
Vermeulen, R.
Vocks, C.
van Weeren, R. J.
Wijers, R. A. M. J.
Wijnands, R.
Wijnholds, S. J.
Wucknitz, O.
Zarka, P.
TI Wide-band, low-frequency pulse profiles of 100 radio pulsars with LOFAR
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; pulsars: general
ID MULTICOMPONENT GAUSSIAN FITS; EMPIRICAL-THEORY; MILLISECOND PULSARS;
INTEGRATED PROFILES; SPECTRAL BEHAVIOR; EMISSION REGION; GEOMETRICAL
ANALYSIS; SUBPULSE MODULATION; DISPERSION MEASURE; AVERAGE PROFILES
AB Context. LOFAR offers the unique capability of observing pulsars across the 10-240MHz frequency range with a fractional bandwidth of roughly 50%. This spectral range is well suited for studying the frequency evolution of pulse profile morphology caused by both intrinsic and extrinsic effects such as changing emission altitude in the pulsar magnetosphere or scatter broadening by the interstellar medium, respectively.
Aims. The magnitude of most of these effects increases rapidly towards low frequencies. LOFAR can thus address a number of open questions about the nature of radio pulsar emission and its propagation through the interstellar medium.
Methods. We present the average pulse profiles of 100 pulsars observed in the two LOFAR frequency bands: high band (120-167MHz, 100 profiles) and low band (15-62MHz, 26 profiles). We compare them with Westerbork Synthesis Radio Telescope (WSRT) and Lovell Telescope observations at higher frequencies (350 and 1400MHz) to study the profile evolution. The profiles were aligned in absolute phase by folding with a new set of timing solutions from the Lovell Telescope, which we present along with precise dispersion measures obtained with LOFAR.
Results. We find that the profile evolution with decreasing radio frequency does not follow a specific trend; depending on the geometry of the pulsar, new components can enter into or be hidden from view. Nonetheless, in general our observations confirm the widening of pulsar profiles at low frequencies, as expected from radius-to-frequency mapping or birefringence theories.
C1 [Pilia, M.; Hessels, J. W. T.; Kondratiev, V. I.; van Leeuwen, J.; Falcke, H.; Sobey, C.; Asgekar, A.; Bentum, M. J.; de Geus, E.; de Jong, A.; Deller, A.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Kuper, G.; Maat, P.; McFadden, R.; Pizzo, R.; Polatidis, A. G.; Tang, Y.; Toribio, M. C.; Vermeulen, R.; Wijnholds, S. J.] ASTRON, Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Pilia, M.; Alexov, A.] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy.
[Hessels, J. W. T.; van Leeuwen, J.; Markoff, S.; van der Horst, A. J.; Wijers, R. A. M. J.; Wijnands, R.] Univ Amsterdam, Anton Pannekoek Inst, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Stappers, B. W.; Kramer, M.; Weltevrede, P.; Lyne, A. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Profsoyuznaya Str 84-32, Moscow 117997, Russia.
[Kramer, M.; Noutsos, A.; Oslowski, S.; Horneffer, A.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Zagkouris, K.; Karastergiou, A.; Broderick, J. W.; Fender, R.; Pietka, M.; Stewart, A.] Univ Oxford, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Hassall, T. E.; Breton, R. P.; Broderick, J. W.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bilous, A. V.; Falcke, H.; ter Veen, S.; Nelles, A.; Thoudam, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Griessmeier, J. -M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45067 Orleans, France.
[Griessmeier, J. -M.; Corbel, S.] Univ Orleans, OSUC, Stn Radioastron Nancay, Observ Paris,CNRS,INSU,USR 704, Route Souesmes, F-18330 Nancay, France.
[Keane, E.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Mail H29,POB 218, Hawthorn, Vic 3122, Australia.
[Keane, E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia.
[Kuniyoshi, M.] Natl Astron Observ Japan, NAOJ Chile Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Oslowski, S.; Schwarz, D.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany.
[Serylak, M.] Univ Western Cape, Dept Phys & Astron, Private Bag X17, ZA-7535 Bellville, South Africa.
[Alexov, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Anderson, J.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum GFZ, Dept Geodesy & Remote Sensing 1, Telegrafenberg A17, D-14473 Potsdam, Germany.
[Asgekar, A.] Shell Technol Ctr, Bangalore 3333, Karnataka, India.
[Avruch, I. M.; Jonker, P.] SRON Netherlands Insitute Space Res, POB 800, NL-9700 AV Groningen, Netherlands.
[Avruch, I. M.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Bell, M. E.; Rowlinson, A.] CSIRO Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia.
[Bentum, M. J.] Univ Twente, NL-7522 Enschede, Netherlands.
[Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Birzan, L.; Garrett, M. A.; Roettgering, H.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Bonafede, A.; Brueggen, M.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Corbel, S.] Univ Paris Diderot, CEA DSM IRFU SAp, CNRS INSU, Lab AIM,CEA IRFU, F-91191 Gif Sur Yvette, France.
[de Geus, E.] SmarterVision BV, Oostersingel 5, NL-9401 JX Assen, Netherlands.
[Eisloeffel, J.] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany.
[Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Lab Lagrange, Observ Cote dAzur,UMR 7293, F-06300 Nice, France.
[Juette, E.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany.
[McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, Sodankyla 99600, Finland.
[McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England.
[Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
[Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Ave Charles Andre, F-69561 St Genis Laval, France.
[Smirnov, O.] Rhodes Univ, Dept Phys & Elelctron, POB 94, ZA-6140 Grahamstown, South Africa.
[Smirnov, O.] SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa.
[Swinbank, J. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Tasse, C.; Zarka, P.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
RP Pilia, M (reprint author), ASTRON, Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.; Pilia, M (reprint author), INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy.
EM pilia@astron.nl
RI Miller-Jones, James/B-2411-2013; Kondratiev, Vladislav/N-1105-2015;
Breton, Rene/A-5536-2017;
OI Deller, Adam/0000-0001-9434-3837; van Weeren,
Reinout/0000-0002-0587-1660; Oslowski, Stefan/0000-0003-0289-0732;
Miller-Jones, James/0000-0003-3124-2814; Kondratiev,
Vladislav/0000-0001-8864-7471; Breton, Rene/0000-0001-8522-4983; Wijers,
Ralph/0000-0002-3101-1808; Bilous, Anna/0000-0002-7177-6987
FU NWO Dynamisering grant; European Commission
[FP7-PEOPLE-2007-4-3-IRG-224838]; RAS, Autonomous Region of Sardinia;
European Research Council under the European Union [337062, 617199];
Alexander von Humboldt Foundation; Agence Nationale de la Recherche
[ANR-09-JCJC-0001-01]
FX M.P. wishes to thank A. Archibald, V. Beskin and J. Dyks for useful
discussion. We are grateful to an anonymous referee whose comments
notably improved the quality of our work. This work was made possible by
an NWO Dynamisering grant to ASTRON, with additional contributions from
European Commission grant FP7-PEOPLE-2007-4-3-IRG-224838 to JVL. LOFAR,
the Low-Frequency Array designed and constructed by ASTRON, has
facilities in several countries, that are owned by various parties (each
with their own funding sources), and that are collectively operated by
the International LOFAR Telescope (ILT) foundation under a joint
scientific policy. M.P. acknowledges financial support from the RAS,
Autonomous Region of Sardinia. J.W.T.H., V.I.K. and J.V.L. acknowledge
support from the European Research Council under the European Union's
Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nrs.
337062 (JWTH, VIK) and 617199 (JVL). SO is supported by the Alexander
von Humboldt Foundation. C. Ferrari acknowledges financial support by
the "Agence Nationale de la Recherche" through grant
ANR-09-JCJC-0001-01.
NR 90
TC 8
Z9 8
U1 1
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A92
DI 10.1051/0004-6361/201425196
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900103
ER
PT J
AU Spezzano, S
Gupta, H
Brunken, S
Gottlieb, CA
Caselli, P
Menten, KM
Muller, HSP
Bizzocchi, L
Schilke, P
McCarthy, MC
Schlemmer, S
AF Spezzano, S.
Gupta, H.
Bruenken, S.
Gottlieb, C. A.
Caselli, P.
Menten, K. M.
Mueller, H. S. P.
Bizzocchi, L.
Schilke, P.
McCarthy, M. C.
Schlemmer, S.
TI A study of the C3H2 isomers and isotopologues: first interstellar
detection of HDCCC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; line: identification; ISM: molecules; ISM: clouds
ID CARBON-CHAIN-CHEMISTRY; DEUTERATED MOLECULES; ASTRONOMICAL DETECTION;
SMALL HYDROCARBONS; ABUNDANCE RATIO; CLOUDS; H2CCC; PROPADIENYLIDENE;
CORES; TMC-1
AB The partially deuterated linear isomer HDCCC of the ubiquitous cyclic carbene (c-C3H2) was observed in the starless cores TMC-1C and L1544 at 96.9 GHz, and a confirming line was observed in TMC-1 at 19.38 GHz. To aid the identification in these narrow line sources, four centimetre-wave rotational transitions (two in the previously reported K-a = 0 ladder and two new ones in the K-a = 1 ladder) and 23 transitions in the millimetre band between 96 and 272 GHz were measured in high-resolution laboratory spectra. Ten spectroscopic constants in a standard asymmetric top Hamiltonian allow the main transitions of astronomical interest in the K-a <= 3 rotational ladders to be calculated to within 0.1 km s(-1) in radial velocity up to 400 GHz. Conclusive identification of the two astronomical lines of HDCCC was provided by the VLSR, which is the same as for the normal isotopic species (H2CCC) in the three narrow line sources. In these sources, deuterium fractionation in singly substituted H2CCC (HDCCC/H2CCC similar to 4-19%) is comparable to that in c-C3H2 (c-C3H2/c-C3HD similar to 5-17%) and similarly in doubly deuterated c-C3H2 (c-C3D2/c-C3HD similar to 3-17%), implying that the efficiency of the deuteration processes in the H2CCC and c-C3H2 isomers are comparable in dark clouds.
C1 [Spezzano, S.; Caselli, P.; Bizzocchi, L.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Gupta, H.] CALTECH, 770 S Wilson Ave,M-C 100-22, Pasadena, CA 91125 USA.
[Spezzano, S.; Bruenken, S.; Mueller, H. S. P.; Schilke, P.; Schlemmer, S.] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany.
[Gottlieb, C. A.; McCarthy, M. C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gottlieb, C. A.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Gupta, H.] Natl Sci Fdn, Div Astron Sci, 4201 Wilson Blvd,Suite 1045, Arlington, VA 22230 USA.
RP Spezzano, S (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM spezzano@mpe.mpg.de
RI Brunken, Sandra/B-1880-2010; Schlemmer, Stephan/E-2903-2015
OI Brunken, Sandra/0000-0001-7175-4828; Schlemmer,
Stephan/0000-0002-1421-7281
FU Deutsche Forschungsgemeinschaft (DFG); NASA [NNX13AE59G]; Bonn Cologne
Graduate School of Physics and Astronomy (BCGS)
FX This work is carried out within the Collaborative Research Centre 956,
sub-project [B2], funded by the Deutsche Forschungsgemeinschaft (DFG),
and has also been supported by the NASA grant NNX13AE59G. S. Spezzano
wishes to thank the Bonn Cologne Graduate School of Physics and
Astronomy (BCGS) for financial support. Any opinions, findings, and
conclusions in this article are those of the authors and do not
necessarily reflect the views of the National Science Foundation.
NR 48
TC 4
Z9 4
U1 4
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A110
DI 10.1051/0004-6361/201527460
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900121
ER
PT J
AU Trabert, E
Beiersdorfer, P
Brickhouse, NS
Golub, L
AF Traebert, Elmar
Beiersdorfer, Peter
Brickhouse, Nancy S.
Golub, Leon
TI Low-density laboratory spectra near the He II lambda 304 line
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; atomic data; methods: laboratory: atomic; techniques:
spectroscopic; Sun: UV radiation
ID EXTREME-ULTRAVIOLET REGION; AN ATOMIC DATABASE; BEAM ION-TRAP;
EMISSION-LINES; CORONAL LINES; AR-XIV; FE-VII; CHIANTI; ANGSTROM;
INSTRUMENT
AB Aims. To interpret the EUV spectra of the solar corona, one hopes for laboratory data of specific chemical elements obtained under coronal conditions.
Methods. EUV spectra of He, C, N, O, F, Ne, S, Ar, Fe, and Ni in a 40 angstrom wide wavelength interval near lambda 304 were excited in an electron beam ion trap.
Results. We observe some two hundred lines about half of which are not yet identified and included in spectral models.
Conclusions. Our data provide a check on the atomic data bases underlying the spectral models that are used to interpret solar corona data. However, a multitude of mostly weak additional lines taken together represent a flux that is comparable to that of various primary lines.
C1 [Traebert, Elmar; Beiersdorfer, Peter] Lawrence Livermore Natl Lab, Div Phys, Phys & Life Sci, Livermore, CA 94550 USA.
[Traebert, Elmar] Ruhr Univ Bochum, Astron Inst, Fak Phys, D-44780 Bochum, Germany.
[Brickhouse, Nancy S.; Golub, Leon] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Trabert, E; Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, Div Phys, Phys & Life Sci, Livermore, CA 94550 USA.; Trabert, E (reprint author), Ruhr Univ Bochum, Astron Inst, Fak Phys, D-44780 Bochum, Germany.
EM traebert@astro.rub.de; beiersdorfer1@llnl.gov
FU US Department of Energy by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; German Research Association (DFG) [Tr171/18,
Tr171/19]
FX This work was performed under the auspices of the US Department of
Energy by Lawrence Livermore National Laboratory under Contract
DE-AC52-07NA27344. E.T. acknowledges support from the German Research
Association (DFG) (grants Tr171/18 and Tr171/19).
NR 32
TC 0
Z9 0
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2016
VL 586
AR A115
DI 10.1051/0004-6361/201527825
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1XG
UT WOS:000369715900126
ER
PT J
AU Baugh, AT
Ryan, MJ
Bernal, XE
Rand, AS
Bee, MA
AF Baugh, Alexander T.
Ryan, Michael J.
Bernal, Ximena E.
Rand, A. Stanley
Bee, Mark A.
TI Female Tungara Frogs Do Not Experience the Continuity Illusion
SO BEHAVIORAL NEUROSCIENCE
LA English
DT Article
DE auditory induction; continuity illusion; perceptual restoration;
Physalaemus pustulosus; temporal induction
ID SENSORY-PERCEPTUAL TRANSFORMATIONS; HEARING ILLUSORY SOUNDS; PRIMARY
AUDITORY-CORTEX; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; MATE CHOICE;
RECEIVER PERMISSIVENESS; ANURAN AMPHIBIANS; MATING SIGNALS; NOISE
AB In humans and some nonhuman vertebrates, a sound containing brief silent gaps can be rendered perceptually continuous by inserting noise into the gaps. This so-called "continuity illusion" arises from a phenomenon known as "auditory induction" and results in the perception of complete auditory objects despite fragmentary or incomplete acoustic information. Previous studies of auditory induction in gray treefrogs (Hyla versicolor and H. chrysoscelis) have demonstrated an absence of this phenomenon. These treefrog species produce pulsatile (noncontinuous) vocalizations, whereas studies of auditory induction in other taxa, including humans, often present continuous sounds (e.g., frequency-modulated sweeps). This study investigated the continuity illusion in a frog (Physalaemus pustulosus) with an advertisement vocalization that is naturally continuous and thus similar to the tonal sweeps used in human psychophysical studies of auditory induction. In a series of playback experiments, female subjects were presented with sets of stimuli that included complete calls, calls with silent gaps, and calls with silent gaps filled with noise. The results failed to provide evidence of auditory induction. Current evidence, therefore, suggests that mammals and birds experience auditory induction, but frogs may not. This emerging pattern of taxonomic differences is considered in light of potential methodological, neurophysiological, and functional explanations.
C1 [Baugh, Alexander T.] Swarthmore Coll, Dept Biol, 500 Coll Ave, Swarthmore, PA 19081 USA.
[Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA.
[Ryan, Michael J.; Bernal, Ximena E.; Rand, A. Stanley] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
[Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA.
[Bee, Mark A.] Univ Minnesota Twin Cities, Dept Ecol Evolut & Behav, St Paul, MN USA.
RP Baugh, AT (reprint author), Swarthmore Coll, Dept Biol, 500 Coll Ave, Swarthmore, PA 19081 USA.
EM abaugh1@swarthmore.edu
OI Bee, Mark A./0000-0002-6770-9730; Baugh, Alexander/0000-0003-2032-892X
FU NSF [IOB 0544096]; NIH [R01DC009582]
FX This work was supported by NSF IOB 0544096 (Michael J. Ryan) and NIH
R01DC009582 (Mark A. Bee). We thank the Smithsonian Tropical Research
Institute for providing logistical support and interns for assisting in
data collection. Autoridad Nacional del Ambiente approved scientific
permits in the Republic of Panama.
NR 78
TC 0
Z9 0
U1 4
U2 10
PU AMER PSYCHOLOGICAL ASSOC
PI WASHINGTON
PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA
SN 0735-7044
EI 1939-0084
J9 BEHAV NEUROSCI
JI Behav. Neurosci.
PD FEB
PY 2016
VL 130
IS 1
BP 62
EP 74
DI 10.1037/bne0000115
PG 13
WC Behavioral Sciences; Neurosciences
SC Behavioral Sciences; Neurosciences & Neurology
GA DE6LK
UT WOS:000370745000008
PM 26692450
ER
PT J
AU Ostorero, L
Morganti, R
Diaferio, A
Siemiginowska, A
Stawarz, L
Moderski, R
Labiano, A
AF Ostorero, L.
Morganti, R.
Diaferio, A.
Siemiginowska, A.
Stawarz, L.
Moderski, R.
Labiano, A.
TI N-H-N-HI correlation in gigahertz-peaked-spectrum galaxies
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE galaxies: active; galaxies: ISM; ISM: clouds; radio lines: galaxies;
X-rays: galaxies
ID COMPACT RADIO GALAXIES; BROAD-BAND SPECTRA; X-RAY-PROPERTIES;
STEEP-SPECTRUM; ABSORBING GAS; ABSORPTION; GPS; SAMPLE; JETS; VIEW
AB With the Westerbork Synthesis Radio Telescope, we performed H-I observations of a sample of known X-ray emitting Gigahertz-peaked-spectrum galaxies with compact-symmetric-object morphology (GPS/CSOs) that lacked an H-I absorption detection. We combined radio and X-ray data of the full sample of X-ray emitting GPS/CSOs and found a significant, positive correlation between the column densities of the total and neutral hydrogen (N-H and N-HI, respectively). Using a Bayesian approach, we simultaneously quantified the parameters of the N-H - N-HI relation and the intrinsic spread of the data set. For a specific subset of our sample, we found N-H proportional to N-HI(b), with b = 0.93(-0.33)(+0.49), and sigma(int)(N-H) = 1.27(-0.40)(+1.30). The N-H-N-HI correlation suggests a connection between the physical properties of the radio and X-ray absorbing gas. (C) 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
C1 [Ostorero, L.; Diaferio, A.] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy.
[Ostorero, L.; Diaferio, A.] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy.
[Morganti, R.] Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Morganti, R.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland.
[Moderski, R.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
[Labiano, A.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
RP Ostorero, L (reprint author), Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy.; Ostorero, L (reprint author), Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy.
EM ostorero@ph.unito.it
FU European Commission [283393]; "Helena Kluyver" programme by ASTRON/JIVE;
INFN grant INDARK; Italian Ministry of University and Research;
University of Torino; Compagnia di San Paolo; Department of Physics and
Astronomy of the University of Pennsylvania; High Energy Astrophysics
Division of the Harvard-Smithsonian Center for Astrophysics; Polish
National Science Centre [DEC-2012/04/A/ST9/00083]; Netherlands
Foundation for Scientific Research (NWO)
FX We thank the organisers of the Fifth Workshop on CSS and GPS sources for
an extremely stimulating and enjoyable meeting. The research leading to
these results has received funding from the European Commission Seventh
Framework Programme (FP/2007-2013) under grant agreement No 283393
(RadioNet3). L.O. acknowledges support from the "Helena Kluyver"
programme run by ASTRON/JIVE, the INFN grant INDARK, the grant PRIN 2012
"Fisica Astroparticellare Teorica" of the Italian Ministry of University
and Research, and the "Strategic Research Grant: Origin and Detection of
Galactic and Extragalactic Cosmic Rays" funded by the University of
Torino and Compagnia di San Paolo. L.O. is grateful to the Department of
Physics and Astronomy of the University of Pennsylvania and to the High
Energy Astrophysics Division of the Harvard-Smithsonian Center for
Astrophysics for their support and kind hospitality. L.S. was supported
by the Polish National Science Centre through the grant
DEC-2012/04/A/ST9/00083. We are grateful to G.Jozsa for his support
during the observing runs with the WSRT and for providing us with the
data-cubes of our target sources. We thank J. Buchner and M. Gruberbauer
for developing their superb code APEMoST and making it available to the
community. S. Andreon is acknowledged for a very stimulating seminar on
Bayesian statistics. The WSRT is operated by ASTRON (Netherlands
Institute for Radio Astronomy) with support from the Netherlands
Foundation for Scientific Research (NWO).
NR 32
TC 1
Z9 1
U1 0
U2 1
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 0004-6337
EI 1521-3994
J9 ASTRON NACHR
JI Astro. Nachr.
PD FEB
PY 2016
VL 337
IS 1-2
BP 148
EP 153
DI 10.1002/asna.201512284
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD8BA
UT WOS:000370147600025
ER
PT J
AU O'Dea, CP
Siemiginowska, A
AF O'Dea, C. P.
Siemiginowska, A.
TI Summary
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE galaxies: active; galaxies: ISM; galaxies: jets; history and philosophy
of astronomy
ID STEEP-SPECTRUM SOURCES; SOURCE PMN J1603-4904; GALAXY; AGN
C1 [O'Dea, C. P.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
[O'Dea, C. P.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA.
[Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP O'Dea, CP (reprint author), Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.; O'Dea, CP (reprint author), Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 0004-6337
EI 1521-3994
J9 ASTRON NACHR
JI Astro. Nachr.
PD FEB
PY 2016
VL 337
IS 1-2
BP 205
EP 208
DI 10.1002/asna.201512281
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD8BA
UT WOS:000370147600035
ER
PT J
AU Blanchard, PK
Berger, E
Fong, WF
AF Blanchard, Peter K.
Berger, Edo
Fong, Wen-fai
TI THE OFFSET AND HOST LIGHT DISTRIBUTIONS OF LONG GAMMA-RAY BURSTS: A NEW
VIEW FROM HST OBSERVATIONS OF SWIFT BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general
ID CORE-COLLAPSE SUPERNOVAE; LUMINOSITY FUNCTIONS; STAR-FORMATION;
SUPERLUMINOUS SUPERNOVAE; ABUNDANCE GRADIENTS; SPIRAL GALAXIES;
FORMATION RATES; MASSIVE STARS; DEEP FIELD; PROGENITORS
AB We present the results of an extensive Hubble Space Telescope imaging study of 105, mostly Swift, long-duration gamma-ray bursts (LGRBs) spanning 0.03 less than or similar to z less than or similar to 9.4, which were localized using relative astrometry from ground-and space-based afterglow observations. We measure the distribution of LGRB offsets from their host centers and their relation to the underlying host light distribution. We find that the host-normalized offsets of LGRBs are more centrally concentrated than expected for an exponential disk profile, < R/R-h > = 0.63, and in particular they are more concentrated than the underlying surface brightness profiles of their host galaxies and more concentrated than supernovae. The fractional flux distribution, with a median of 0.78, indicates that LGRBs prefer some of the brightest locations in their host galaxies but are not as strongly correlated as previous studies indicated. Importantly, we find a clear correlation between offset and fractional flux, where bursts at offsets R/R-h less than or similar to 0.5 exclusively occur at fractional fluxes greater than or similar to 0.6, while bursts at R/R-h greater than or similar to 0.5 have a uniform fractional flux distribution. This indicates that the spatial correlation of LGRBs with bright star-forming regions seen in the full sample is dominated by the contribution from bursts at small offset and that LGRBs in the outer parts of galaxies show no preference for unusually bright regions. We conclude that LGRBs strongly prefer the bright, inner regions of their hosts, indicating that the star formation taking place there is more favorable for LGRB progenitor production. This indicates that environmental factors beyond metallicity, such as binary interactions or IMF differences, may operate in the central regions of LGRB hosts.
C1 [Blanchard, Peter K.; Berger, Edo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fong, Wen-fai] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
RP Blanchard, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM pblanchard@cfa.harvard.edu
FU NSF [AST-1411763]; NASA [NNX15AE50G, NAS5-26555]; National Science
Foundation Graduate Research Fellowship [DGE1144152]; NASA through
Einstein Postdoctoral Fellowship [PF4-150121, NAS8-03060]; NASA Office
of Space Science [NNX09AF08G]
FX The Berger GRB group at Harvard is supported in part by the NSF under
grant AST-1411763 and by NASA under grant NNX15AE50G. This paper is
based upon work supported by the National Science Foundation Graduate
Research Fellowship Program under Grant No. DGE1144152. W.F.
acknowledges support provided by NASA through Einstein Postdoctoral
Fellowship grant number PF4-150121 issued by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060. We thank Ragnhild
Lunnan, Maria Drout, Josh Grindlay, and Avi Loeb for helpful
discussions. The HST data presented here and the Swift/UVOT data used in
this work were obtained from the Mikulski Archive for Space Telescopes
(MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for
MAST for non-HST data is provided by the NASA Office of Space Science
via grant NNX09AF08G and by other grants and contracts. Based in part on
observations obtained at the Gemini Observatory, acquired through the
Gemini Science Archive, and processed using the Gemini IRAF package,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under a cooperative agreement with the NSF on behalf of
the Gemini partnership: the National Science Foundation (United States),
the National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia, Tecnologia e
Inovacao (Brazil) and Ministerio de Ciencia, Tecnologi'a e Innovacion
Productiva (Argentina). Based in part on data obtained from the ESO
Science Archive Facility. This paper makes use of data gathered with the
6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
This research has made use of data obtained from the Chandra Data
Archive and software provided by the Chandra X-ray Center (CXC) in the
application package CIAO. Based in part on data collected at the Subaru
Telescope and obtained from SMOKA, which is operated by the Astronomy
Data Center, National Astronomical Observatory of Japan. We thank S.B.
Cenko for providing Palomar 60 inch afterglow images for GRBs 060206 and
090618, T. Kruhler and J. Greiner for providing GROND afterglow images
for GRBs 080520, 081121, and 081109 and a WHT image for GRB 090113, D.
Malesani for providing a TNG afterglow image for GRB 060605, D. A. Kann
for providing a WHT afterglow image for GRB 060124, and D. Perley for
providing a Keck telescope afterglow image of GRB 071010A and a Palomar
60 inch afterglow image of GRB 080607.
NR 58
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2016
VL 817
IS 2
AR 144
DI 10.3847/0004-637X/817/2/144
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900061
ER
PT J
AU Brogi, M
de Kok, RJ
Albrecht, S
Snellen, IAG
Birkby, JL
Schwarz, H
AF Brogi, M.
de Kok, R. J.
Albrecht, S.
Snellen, I. A. G.
Birkby, J. L.
Schwarz, H.
TI ROTATION AND WINDS OF EXOPLANET HD 189733 b MEASURED WITH
HIGH-DISPERSION TRANSMISSION SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: fundamental
parameters; planets and satellites: individual (HD 189733 b);
techniques: spectroscopic
ID HUBBLE-SPACE-TELESCOPE; COLLISION-INDUCED ABSORPTION; TIDALLY LOCKED
EXOPLANETS; UPSILON ANDROMEDAE B; TAU BOOTIS B; EXTRASOLAR PLANET; HOT
JUPITERS; MU-M; ATMOSPHERIC CIRCULATION; PHASE CURVES
AB Giant exoplanets orbiting very close to their parent star (hot Jupiters) are subject to tidal forces expected to synchronize their rotational and orbital periods on short timescales (tidal locking). However, spin rotation has never been measured directly for hot Jupiters. Furthermore, their atmospheres can show equatorial super-rotation via strong eastward jet streams, and/or high-altitude winds flowing from the day-to the night-side hemisphere. Planet rotation and atmospheric circulation broaden and distort the planet spectral lines to an extent that is detectable with measurements at high spectral resolution. We observed a transit of the hot Jupiter HD 189733 b around 2.3 mu m and at a spectral resolution of R similar to 10(5) with CRIRES at the ESO Very Large Telescope. After correcting for the stellar absorption lines and their distortion during transit (the Rossiter-McLaughlin effect), we detect the absorption of carbon monoxide and water vapor in the planet transmission spectrum by cross-correlating with model spectra. The signal is maximized (7.6 sigma) for a planet rotational velocity of (3.4(-2.1)(+1.3)) km s(-1), corresponding to a rotational period of (1.7(-0.4)(+2.9)) days. This is consistent with the planet orbital period of 2.2 days, and therefore with tidal locking. We find that the rotation of HD. 189733 b is longer than 1 day (3 sigma). The data only marginally (1.5 sigma) prefer models with rotation versus models without rotation. We measure a small day-to night-side wind speed of (-1.7(-1.2)(+1.1)) km s(-1). Compared to the recent detection of sodium blueshifted by (8 +/- 2) km s(-1), this likely implies a strong vertical wind shear between the pressures probed by near-infrared and optical transmission spectroscopy.
C1 [Brogi, M.] Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA.
[de Kok, R. J.; Snellen, I. A. G.; Schwarz, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[de Kok, R. J.] SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Albrecht, S.] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Birkby, J. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Brogi, M (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA.
EM matteo.brogi@colorado.edu
FU NASA - Space Telescope Science Institute [HST-HF2-51336]; NASA;
Netherlands Organization for Scientific Research (NWO) [VICI
639.043.107]; Danish National Research Foundation [DNRF106]; ESO Very
Large Telescope [289.C-5030]
FX This work is based on data collected at the ESO Very Large Telescope
during the DDT program 289.C-5030. We are grateful to the ESO staff at
Paranal for the help in performing these observations.; M.B.
acknowledges support by NASA, through Hubble Fellowship grant
HST-HF2-51336 awarded by the Space Telescope Science Institute.; This
work was performed in part under contract with the California Institute
of Technology (Caltech)/Propulsion Laboratory (JPL) funded by NASA
through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute.; This work is part of the research programs PEPSci
and VICI 639.043.107, which are financed by the Netherlands Organization
for Scientific Research (NWO).; Funding for the Stellar Astrophysics
Centre is provided by the Danish National Research Foundation (grant
DNRF106).
NR 81
TC 8
Z9 8
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2016
VL 817
IS 2
AR 106
DI 10.3847/0004-637X/817/2/106
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900023
ER
PT J
AU Gao, F
Braatz, JA
Reid, MJ
Lo, KY
Condon, JJ
Henkel, C
Kuo, CY
Impellizzeri, CMV
Pesce, DW
Zhao, W
AF Gao, F.
Braatz, J. A.
Reid, M. J.
Lo, K. Y.
Condon, J. J.
Henkel, C.
Kuo, C. Y.
Impellizzeri, C. M. V.
Pesce, D. W.
Zhao, W.
TI THE MEGAMASER COSMOLOGY PROJECT. VIII. A GEOMETRIC DISTANCE TO NGC 5765b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; dark energy; distance scale; galaxies:
individual (NGC 5765b); galaxies: nuclei; masers
ID ANGULAR-DIAMETER DISTANCE; ACTIVE GALAXY NGC-4258; HUBBLE CONSTANT; UGC
3789; SPIRAL STRUCTURE; MASER EMISSION; ACCRETION DISK; WATER MASERS;
BLACK-HOLE; ACCELERATIONS
AB As part of the Megamaser Cosmology Project, here we present a new geometric distance measurement to the megamaser galaxy NGC 5765b. Through a series of very long baseline interferometry observations, we have confirmed the water masers trace a thin, sub-parsec Keplerian disk around the nucleus, implying an enclosed mass of 4.55 +/- 0.40 x 10(7) M-circle dot. Meanwhile, from single-dish monitoring of the maser spectra over two years, we measured the secular drifts of maser features near the systemic velocity of the galaxy with rates between 0.5 and 1.2 km s(-1) yr(-1). Fitting a warped, thin-disk model to these measurements, we determine a Hubble Constant H-0 of 66.0 +/- 6.0 km s(-1) Mpc(-1) with an. angular-diameter distance to NGC 5765b of 126.3 +/- 11.6 Mpc. Apart from the distance measurement, we also investigate some physical properties related to the maser disk in NGC 5765b. The high-velocity features are spatially distributed into several clumps, which may indicate the existence of a spiral density wave associated with the accretion disk. For the redshifted features, the envelope defined by the peak maser intensities increases with radius. The profile of the systemic masers in NGC 5765b is smooth and shows almost no structural changes over the two years of monitoring time, which differs from the more variable case of NGC 4258.
C1 [Gao, F.; Zhao, W.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China.
[Gao, F.; Braatz, J. A.; Lo, K. Y.; Condon, J. J.; Impellizzeri, C. M. V.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Gao, F.] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China.
[Reid, M. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Henkel, C.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Henkel, C.] King Abdulaziz Univ, POB 80203, Jeddah 21413, Saudi Arabia.
[Kuo, C. Y.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Impellizzeri, C. M. V.] Joint Alma Off, Alsonso de Cordova 3107, Santiago, Chile.
[Pesce, D. W.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
RP Gao, F (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China.; Gao, F (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.; Gao, F (reprint author), Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China.
FU National Radio Astronomy Observatory (NRAO) through the Grote Reber
Doctoral Fellowship; Major Program of National Natural Science
Foundation of China [11590780, 11590784]; Strategic Priority Research
Program "The Emergence of Cosmological Structures" of the Chinese
Academy of Sciences [XDB09000000]
FX We thank the anonymous referee for valuable comments on the paper. F.G.
gratefully acknowledges support provided by the National Radio Astronomy
Observatory (NRAO) through the Grote Reber Doctoral Fellowship, and
support in part by the Major Program of National Natural Science
Foundation of China (grants 11590780 and 11590784) and the Strategic
Priority Research Program "The Emergence of Cosmological Structures" of
the Chinese Academy of Sciences, grant No. XDB09000000. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. This research has made use of the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900045
ER
PT J
AU Jee, MJ
Dawson, WA
Stroe, A
Wittman, D
van Weeren, RJ
Bruggen, M
Bradac, M
Rottgering, H
AF Jee, M. James
Dawson, William A.
Stroe, Andra
Wittman, David
van Weeren, Reinout J.
Brueggen, Marcus
Bradac, Marusa
Rottgering, Huub
TI MC2: MAPPING THE DARK MATTER DISTRIBUTION OF THE "TOOTHBRUSH" CLUSTER RX
J0603.3+4214 WITH HUBBLE SPACE TELESCOPE AND SUBARU WEAK LENSING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark matter; galaxies: clusters: individual (RX
J0603.3+4214); galaxies: high-redshift; gravitational lensing: weak;
X-rays: galaxies: clusters
ID DIFFUSE RADIO-EMISSION; MERGING GALAXY CLUSTER; EL GORDO;
PARTICLE-ACCELERATION; CIZA J2242.8+5301; RELICS; MERGERS; CORE;
LUMINOSITY; COSMOLOGY
AB The galaxy cluster RX J0603.3+4214. at z-0.225 is one of the rarest clusters boasting an extremely large (similar to 2 Mpc) radio. relic. Because of the remarkable morphology of the relic, the cluster is nicknamed the. "Toothbrush Cluster." Although the cluster's underlying mass distribution is one of the critical pieces of information needed to reconstruct the merger scenario responsible for the puzzling radio. relic morphology, its proximity to the Galactic plane b similar to 10 degrees has imposed significant observational challenges. We present a high-resolution weak-lensing study of the cluster with Subaru/Suprime Cam and Hubble Space Telescope imaging data. Our mass reconstruction reveals that the cluster is composed of complicated dark matter substructures closely tracing the galaxy distribution, in contrast, however, with the relatively simple binary X-ray morphology. Nevertheless, we find that the cluster mass is still dominated by the two most massive clumps aligned north-south with a similar to 3: 1 mass ratio (M-200 = 6.29(-1.62)(+2.24) x 10(14) M-circle dot and 1.98(-0.74)(+1.24) x 10(14) M-circle dot for the northern and southern clumps, respectively). The southern mass peak is similar to 2' offset toward the south with respect to the corresponding X-ray peak, which has a "bullet"-like morphology pointing south. Comparison of the current weak-lensing result with the X-ray, galaxy, and radio. relic suggests that perhaps the dominant mechanism responsible for the observed relic may be a highspeed collision of the two most massive subclusters, although the peculiarity of the morphology necessitates involvement of additional subclusters. Careful numerical simulations should follow in order to obtain more complete understanding of the merger scenario utilizing all existing observations.
C1 [Jee, M. James] Yonsei Univ, Dept Astron, 50 Yonsei Ro, Seoul 03722, South Korea.
[Jee, M. James] Yonsei Univ, Ctr Galaxy Evolut Res, 50 Yonsei Ro, Seoul 03722, South Korea.
[Jee, M. James; Wittman, David; Bradac, Marusa] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA.
[Dawson, William A.] Lawrence Livermore Natl Lab, POB 808 L-210, Livermore, CA 94551 USA.
[Stroe, Andra; Rottgering, Huub] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[van Weeren, Reinout J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Brueggen, Marcus] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
RP Jee, MJ (reprint author), Yonsei Univ, Dept Astron, 50 Yonsei Ro, Seoul 03722, South Korea.; Jee, MJ (reprint author), Yonsei Univ, Ctr Galaxy Evolut Res, 50 Yonsei Ro, Seoul 03722, South Korea.; Jee, MJ (reprint author), Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA.
OI van Weeren, Reinout/0000-0002-0587-1660
FU NASA through a grant from the Space Telescope Science Institute
[HST-GO-13343.01-A]; NRF of Korea; NWO top subsidy [614.001.006];
European Research Council under the European Unions Seventh Framework
Programme (FP)/ERC Advanced Grant [NewClusters-321271]; U.S. DOE
[DE-AC52-07NA27344]
FX Support for Program number HST-GO-13343.01-A was provided by NASA
through a grant from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Incorporated, under NASA contract NAS5-26555. M.J.J. acknowledges
support from NRF of Korea to CGER. A.S. acknowledges financial support
from an NWO top subsidy (614.001.006). H.R. gratefully acknowledges
support from the European Research Council under the European Unions
Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant
NewClusters-321271. Part of this work was performed under the auspices
of the U.S. DOE by LLNL under Contract DE-AC52-07NA27344.
NR 56
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900096
ER
PT J
AU Kozlowski, S
Kochanek, CS
Ashby, MLN
Assef, RJ
Brodwin, M
Eisenhardt, PR
Jannuzi, BT
Stern, D
AF Kozlowski, Szymon
Kochanek, Christopher S.
Ashby, Matthew L. N.
Assef, Roberto J.
Brodwin, Mark
Eisenhardt, Peter R.
Jannuzi, Buell T.
Stern, Daniel
TI QUASAR VARIABILITY IN THE MID-INFRARED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: active; infrared: galaxies; quasars:
general
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS;
SPITZER-SPACE-TELESCOPE; DAMPED RANDOM-WALK; WIDE-FIELD SURVEY;
SUPERMASSIVE BLACK-HOLES; LARGE-MAGELLANIC-CLOUD; ARRAY CAMERA IRAC;
X-RAY SOURCES; OPTICAL VARIABILITY
AB The Decadal IRAC Bootes Survey is a mid-IR variability survey of the similar to 9 sq. deg. of the NDWFS Bootes Field and extends the time baseline of its predecessor, the Spitzer Deep, Wide-Field Survey (SDWFS), from 4 to 10 years. The Spitzer Space Telescope visited the field five times between 2004 and 2014 at 3.6 and 4.5 mu m. We provide the difference image analysis photometry for a half a million mostly extragalactic sources. In mid-IR color-color plane, sources with quasar colors constitute the largest variability class (75%), 16% of the variable objects have stellar colors and the remaining 9% have the colors of galaxies. Adding the fifth epoch doubles the number of variable active galactic nuclei (AGNs) for the same false positive rates as in SDWFS, or increases the number of sources by 20% while decreasing the false positive rates by factors of 2-3 for the same variability amplitude. We quantify the ensemble mid-IR variability of similar to 1500 spectroscopically confirmed AGNs using single power-law structure functions (SFs), which we find to be steeper (index gamma approximate to 0.45) than in the optical (gamma approximate to 0.3), leading to much lower amplitudes at short time-lags. This provides evidence for large emission regions, smoothing out any fast UV/optical variations, as the origin of infrared quasar variability. The mid-IR AGN SF slope gamma seems to be uncorrelated with both the luminosity and rest-frame wavelength, while the amplitude shows an anti-correlation with the luminosity and a correlation with the rest-frame wavelength.
C1 [Kozlowski, Szymon] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Kochanek, Christopher S.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito Libertador 441, Santiago, Chile.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Eisenhardt, Peter R.; Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Jannuzi, Buell T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Kozlowski, S (reprint author), Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.; Kochanek, CS (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.; Kochanek, CS (reprint author), Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
EM simkoz@astrouw.edu.pl; kochanek.1@osu.edu
FU Polish National Science Center [2014/15/B/ST9/00093]; Gemini-CONICYT
[32120009]; FONDECYT [1151408]
FX We thank Prof. Igor Soszynski for discussions on variable stars and the
anonymous referee for helpful suggestions that improved the manuscript.
This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of the Technology under contract with the National
Aeronautics and Space Administration (NASA). S.K. acknowledges the
financial support of the Polish National Science Center through the
grant number 2014/15/B/ST9/00093. R.J.A. was supported by Gemini-CONICYT
grant number 32120009 and FONDECYT grant number 1151408.
NR 87
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
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PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900036
ER
PT J
AU LaMassa, SM
Urry, CM
Cappelluti, N
Bohringer, H
Comastri, A
Glikman, E
Richards, G
Ananna, T
Brusa, M
Cardamone, C
Chon, G
Civano, F
Farrah, D
Gilfanov, M
Green, P
Komossa, S
Lira, P
Makler, M
Marchesi, S
Pecoraro, R
Ranalli, P
Salvato, M
Schawinski, K
Stern, D
Treister, E
Viero, M
AF LaMassa, Stephanie M.
Urry, C. Megan
Cappelluti, Nico
Boehringer, Hans
Comastri, Andrea
Glikman, Eilat
Richards, Gordon
Ananna, Tonima
Brusa, Marcella
Cardamone, Carie
Chon, Gayoung
Civano, Francesca
Farrah, Duncan
Gilfanov, Marat
Green, Paul
Komossa, S.
Lira, Paulina
Makler, Martin
Marchesi, Stefano
Pecoraro, Robert
Ranalli, Piero
Salvato, Mara
Schawinski, Kevin
Stern, Daniel
Treister, Ezequiel
Viero, Marco
TI THE 31 DEG(2) RELEASE OF THE STRIPE 82 X-RAY SURVEY: THE POINT SOURCE
CATALOG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies: active; quasars: general; surveys; X-rays: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; DEEP FIELD-SOUTH;
OSCILLATION SPECTROSCOPIC SURVEY; CHANDRA MULTIWAVELENGTH PROJECT;
ATACAMA COSMOLOGY TELESCOPE; INFRARED-SURVEY-EXPLORER; EMISSION-LINE
GALAXIES; 1ST DATA RELEASE; XMM-NEWTON
AB We release the next installment of the Stripe 82 X-ray survey point-source catalog, which currently covers 31.3 deg(2) of the Sloan Digital Sky Survey (SDSS) Stripe 82 Legacy field. In total, 6181 unique X-ray sources are significantly detected with XMM-Newton (>5 sigma) and Chandra (>4.5 sigma). This catalog release includes data from XMM-Newton cycle AO 13, which approximately doubled the Stripe 82X survey area. The flux limits of the Stripe 82X survey are 8.7 x 10(-16) erg s(-1) cm(-2), 4.7 x 10(-15) erg s(-1) cm(-2), and 2.1 x 10(-15) erg s(-1) cm(-2) in the soft (0.5-2 keV), hard (2-10 keV), and full bands (0.5-10 keV), respectively, with approximate half-area survey flux limits of 5.4 x 10(-15) erg s(-1) cm(-2), 2.9 x 10(-14) erg s(-1) cm(-2), and 1.7 x 10(-14) erg s(-1) cm(-2). We matched the X-ray source lists to available multi-wavelength catalogs, including updated matches to the previous release of the Stripe 82X survey; 88% of the sample is matched to a multi-wavelength counterpart. Due to the wide area of Stripe 82X and rich ancillary multi-wavelength data, including coadded SDSS photometry, mid-infrared WISE coverage, near-infrared coverage from UKIDSS and VISTA Hemisphere Survey, ultraviolet coverage from GALEX, radio coverage from FIRST, and far-infrared coverage from Herschel, as well as existing similar to 30% optical spectroscopic completeness, we are beginning to uncover rare objects, such as obscured high-luminosity active galactic nuclei at high-redshift. The Stripe 82X point source catalog is a valuable data set for constraining how this population grows and evolves, as well as for studying how they interact with the galaxies in which they live.
C1 [LaMassa, Stephanie M.; Urry, C. Megan; Ananna, Tonima; Civano, Francesca; Marchesi, Stefano; Pecoraro, Robert] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
[LaMassa, Stephanie M.; Urry, C. Megan; Ananna, Tonima; Pecoraro, Robert] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[LaMassa, Stephanie M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cappelluti, Nico; Comastri, Andrea; Brusa, Marcella; Marchesi, Stefano; Ranalli, Piero] INAF Osservatorio Astronom Bologna, I-40127 Bologna, Italy.
[Boehringer, Hans; Chon, Gayoung; Salvato, Mara] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Richards, Gordon] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Brusa, Marcella] Univ Bologna, DIFA Dipartimento Fis Astron, I-40127 Bologna, Italy.
[Cardamone, Carie] Wheelock Coll, Dept Math & Sci, Boston, MA 02215 USA.
[Civano, Francesca; Green, Paul; Marchesi, Stefano] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Farrah, Duncan] Virginia Polytech Inst & State Univ, Dept Phys MC 0435, Blacksburg, VA 24061 USA.
[Farrah, Duncan] State Univ, Blacksburg, VA 24061 USA.
[Gilfanov, Marat] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Gilfanov, Marat] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Lira, Paulina] Univ Chile, Dept Astron, Santiago, Chile.
[Makler, Martin] Ctr Brasileiro Pesquisas Fis, BR-22290 Rio De Janeiro, Brazil.
[Ranalli, Piero] Natl Observ Athens, Space Applicat & Remote Sensing IAASARS, Inst Astron Astrophys, Penteli 15236, Greece.
[Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schawinski, Kevin] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Viero, Marco] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Viero, Marco] CALTECH, Pasadena, CA 91125 USA.
RP LaMassa, SM (reprint author), Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
RI Makler, Martin/G-2639-2012; Ranalli, Piero/K-6363-2013; Lira,
Paulina/G-8536-2016
OI Makler, Martin/0000-0003-2206-2651; Ranalli, Piero/0000-0003-3956-755X;
FU Yale University; Kavli Institute for Theoretical Physics (Santa
Barbara); NSF [NSF PHY11-25915]; FPY Career Integration Grant "eEASY"
[CIG 321913]; Center of Excellence in Astrophysics and Associated
Technologies [PFB 06]; FONDECYT [1120061]; Anillo project [ACT1101];
Swiss National Science Foundation [PP00P2_138979/1]; Alfred P. Sloan
Foundation; National Science Foundation; U.S. Department of Energy;
National Aeronautics and Space Administration; Japanese Monbukagakusho;
Max Planck Society; Higher Education Funding Council for England;
American Museum of Natural History; Astrophysical Institute Potsdam;
University of Basel; University of Cambridge; Case Western Reserve
University; University of Chicago; Drexel University; Fermilab;
Institute for Advanced Study; Japan Participation Group; Johns Hopkins
University; Joint Institute for Nuclear Astrophysics; Kavli Institute
for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese
Academy of Sciences (LAMOST); Los Alamos National Laboratory;
Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for
Astrophysics (MPA); New Mexico State University; Ohio State University;
University of Pittsburgh; University of Portsmouth; Princeton
University; United States Naval Observatory; University of Washington;
U.S. Department of Energy Office of Science; University of Arizona;
Brazilian Participation Group; Brookhaven National Laboratory; Carnegie
Mellon University; University of Florida; French Participation Group;
German Participation Group; Harvard University; Instituto de Astrofisica
de Canarias; Michigan State/Notre Dame/JINA Participation Group;
Lawrence Berkeley National Laboratory; Max Planck Institute for
Astrophysics; Max Planck Institute for Extraterrestrial Physics; New
York University; Pennsylvania State University; Spanish Participation
Group; University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; [NNX15AJ40G]
FX We thank the anonymous referee for feedback that helped improve the
manuscript. S.M.L. acknowledges support from grant number NNX15AJ40G.
C.M.U. gratefully acknowledges support from Yale University. C.M.U. and
S.K. would like to thank the Kavli Institute for Theoretical Physics
(Santa Barbara) for their hospitality and support; the KITP is supported
by NSF grant No. NSF PHY11-25915. M.B. acknowledges support from the FPY
Career Integration Grant "eEASY" (CIG 321913). Support for the work of
E.T. was provided by the Center of Excellence in Astrophysics and
Associated Technologies (PFB 06), by the FONDECYT grant 1120061 and the
Anillo project ACT1101. K.S. gratefully acknowledges support from Swiss
National Science Foundation Grant PP00P2_138979/1.; Funding for the SDSS
and SDSS-II has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the U.S.
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. The SDSS Web Site is.
http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research
Consortium for the Participating Institutions. The Participating
Institutions are the American Museum of Natural History, Astrophysical
Institute Potsdam, University of Basel, University of Cambridge, Case
Western Reserve University, University of Chicago, Drexel University,
Fermilab, the Institute for Advanced Study, the Japan Participation
Group, Johns Hopkins University, the Joint Institute for Nuclear
Astrophysics, the Kavli Institute for Particle Astrophysics and
Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences
(LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New
Mexico State University, Ohio State University, University of
Pittsburgh, University of Portsmouth, Princeton University, the United
States Naval Observatory, and the University of Washington.; Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. The SDSS-III web site is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, Carnegie Mellon
University, University of Florida, the French Participation Group, the
German Participation Group, Harvard University, the Instituto de
Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University.; This publication makes use of data products from the
Widefield Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900089
ER
PT J
AU Lu, RS
Roelofs, F
Fish, VL
Shiokawa, H
Doeleman, SS
Gammie, CF
Falcke, H
Krichbaum, TP
Zensus, JA
AF Lu, Ru-Sen
Roelofs, Freek
Fish, Vincent L.
Shiokawa, Hotaka
Doeleman, Sheperd S.
Gammie, Charles F.
Falcke, Heino
Krichbaum, Thomas P.
Zensus, J. Anton
TI IMAGING AN EVENT HORIZON: MITIGATION OF SOURCE VARIABILITY OF
SAGITTARIUS A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: individual (Sgr A*); Galaxy: center;
techniques: image processing; techniques: interferometric
ID SUPERMASSIVE BLACK-HOLE; SGR A-ASTERISK; GENERAL-RELATIVISTIC
MAGNETOHYDRODYNAMICS; S ACCRETION FLOW; GALACTIC-CENTER; GRMHD
SIMULATIONS; MILLIMETER-VLBI; CLOSURE PHASES; MODELS; DISKS
AB The black hole in the center of the Galaxy, associated with the compact source Sagittarius A* (Sgr A*), is predicted to cast a shadow upon the emission of the surrounding plasma flow, which encodes the influence of general relativity (GR) in the strong-field regime. The Event Horizon Telescope (EHT) is a Very Long Baseline Interferometry (VLBI) network with a goal of imaging nearby supermassive black holes (in particular Sgr A* and M87) with angular resolution sufficient to observe strong gravity effects near the event horizon. General relativistic magnetohydrodynamic (GRMHD) simulations show that radio emission from Sgr A* exhibits variability on timescales of minutes, much shorter than the duration of a typical VLBI imaging experiment, which usually takes several hours. A changing source structure during the observations, however, violates one of the basic assumptions needed for aperture synthesis in radio interferometry imaging to work. By simulating realistic EHT observations of a model movie of Sgr A*, we demonstrate that an image of the average quiescent emission, featuring the characteristic black hole shadow and photon ring predicted by GR, can nonetheless be obtained by observing over multiple days and subsequent processing of the visibilities (scaling, averaging, and smoothing) before imaging. Moreover, it is shown that this procedure can be combined with an existing method to mitigate the effects of interstellar scattering. Taken together, these techniques allow the black hole shadow in the Galactic center to be recovered on the reconstructed image.
C1 [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA.
[Lu, Ru-Sen; Krichbaum, Thomas P.; Zensus, J. Anton] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Roelofs, Freek; Falcke, Heino] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Shiokawa, Hotaka; Gammie, Charles F.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Lu, RS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA.; Lu, RS (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM rslu@mpifr-bonn.mpg.de
OI Gammie, Charles /0000-0001-7451-8935
FU National Science Foundation [AST-1310896, AST-1211539, AST-1207704,
AST-1440254, AST-1337663]; Gordon and Betty Moore foundation [GBMF-3561]
FX We thank the anonymous referee for comments and suggestions that
improved the quality of the paper. High frequency VLBI work at MIT
Haystack Observatory and Smithsonian Astrophysical Observatory is
supported by grants from the National Science Foundation (AST-1310896,
AST-1211539, AST-1207704, AST-1440254, AST-1337663) and by grant
GBMF-3561 from the Gordon and Betty Moore foundation.
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900090
ER
PT J
AU McDonald, M
Stalder, B
Bayliss, M
Allen, SW
Applegate, DE
Ashby, MLN
Bautz, M
Benson, BA
Bleem, LE
Brodwin, M
Carlstrom, JE
Chiu, I
Desai, S
Gonzalez, AH
Hlavacek-Larrondo, J
Holzapfel, WL
Marrone, DP
Miller, ED
Reichardt, CL
Saliwanchik, BR
Saro, A
Schrabback, T
Stanford, SA
Stark, AA
Vieira, JD
Zenteno, A
AF McDonald, M.
Stalder, B.
Bayliss, M.
Allen, S. W.
Applegate, D. E.
Ashby, M. L. N.
Bautz, M.
Benson, B. A.
Bleem, L. E.
Brodwin, M.
Carlstrom, J. E.
Chiu, I.
Desai, S.
Gonzalez, A. H.
Hlavacek-Larrondo, J.
Holzapfel, W. L.
Marrone, D. P.
Miller, E. D.
Reichardt, C. L.
Saliwanchik, B. R.
Saro, A.
Schrabback, T.
Stanford, S. A.
Stark, A. A.
Vieira, J. D.
Zenteno, A.
TI STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A
TRANSITIONING FUEL SUPPLY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: intracluster medium; galaxies: elliptical and
lenticular, cD; galaxies: starburst; X-rays: galaxies: clusters
ID COOLING FLOW CLUSTERS; GALACTIC NUCLEUS FEEDBACK; X-RAY CAVITIES; SPT-SZ
SURVEY; SOUTH-POLE TELESCOPE; H-ALPHA FILAMENTS; MOLECULAR-HYDROGEN;
THERMAL-INSTABILITY; SPACE-TELESCOPE; INFRARED-SURVEY
AB We present a multiwavelength study of the 90 brightest cluster galaxies (BCGs) in a sample of galaxy clusters selected via the Sunyaev Zel'dovich effect by the South Pole Telescope, utilizing data from various ground- and space-based facilities. We infer the star-formation rate (SFR) for the BCG in each cluster-based on the UV and IR continuum luminosity, as well as the [O II] lambda lambda 3726,3729 emission line luminosity in cases where spectroscopy is available-and find seven systems with SFR > 100 M circle dot yr(-1). We find that the BCG SFR exceeds 10 M circle dot yr(-1) in 31 of 90 (34%) cases at 0.25 < z < 1.25, compared to similar to 1%-5% at z similar to 0 from the literature. At z greater than or similar to 1, this fraction increases to 92(-31)(+6)%, implying a steady decrease in the BCG SFR over the past similar to 9 Gyr. At low-z, we find that the specific SFR in BCGs is declining more slowly with time than for field or cluster galaxies, which is most likely due to the replenishing fuel from the cooling ICM in relaxed, cool core clusters. At z greater than or similar to 0.6, the correlation between the cluster central entropy and BCG star formation-which is well established at z similar to 0-is not present. Instead, we find that the most star-forming BCGs at high-z are found in the cores of dynamically unrelaxed clusters. We use data from the Hubble Space Telescope to investigate the rest-frame near-UV morphology of a subsample of the most star-forming BCGs, and find complex, highly asymmetric UV morphologies on scales as large as similar to 50-60 kpc. The high fraction of star-forming BCGs hosted in unrelaxed, non-cool core clusters at early times suggests that the dominant mode of fueling star formation in BCGs may have recently transitioned from galaxy-galaxy interactions to ICM cooling.
C1 [McDonald, M.; Bautz, M.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Stalder, B.] Univ Hawaii, Inst Astron IFA, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Bayliss, M.; Ashby, M. L. N.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bayliss, M.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
[Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.
[Allen, S. W.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Allen, S. W.] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA.
[Applegate, D. E.; Schrabback, T.] Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
[Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Bleem, L. E.; Carlstrom, J. E.] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Chiu, I.; Desai, S.; Saro, A.] Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Desai, S.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
[Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Saliwanchik, B. R.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA.
[Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA.
[Zenteno, A.] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.
RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mcdonald@space.mit.edu
OI Reichardt, Christian/0000-0003-2226-9169
FU NASA [HST-GO-13456.002A, GO4-15122A, NAS 5-26555, 12800071, 12800088,
13800883]; Hubble Fellowship grant - Space Telescope Science Institute
[HST-HF51308.01-A]; National Science Foundation [ANT-0638937,
PLR-1248097, PHY-1125897]; NSF Physics Frontier Center grant
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF
[AST-1009012, AST-1009649, MRI-0723073]; National Sciences and
Engineering Research Council of Canada; Canada Research Chairs program;
Canadian Institute for Advanced Research; U.S. Department of Energy
[DE-AC02-06CH11357]; University of Melbourne; Australian Research
Councils Discovery Projects scheme [DP150103208]; German Federal
Ministry of Economics and Technology (BMWi) through DLR [50 OR 1210, 50
OR 1308, 50 OR 1407]
FX We thank Mark Voit and John ZuHone for helpful conversations. M.M.
acknowledges support by NASA through contracts HST-GO-13456.002A
(Hubble) and GO4-15122A (Chandra), and Hubble Fellowship grant
HST-HF51308.01-A awarded by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555. The South Pole
Telescope program is supported by the National Science Foundation
through grants ANT-0638937 and PLR-1248097. Partial support is also
provided by the NSF Physics Frontier Center grant PHY-0114422 to the
Kavli Institute of Cosmological Physics at the University of Chicago,
the Kavli Foundation, and the Gordon and Betty Moore Foundation. Support
for X-ray analysis was provided by NASA through Chandra Award Numbers
12800071, 12800088, and 13800883 issued by the Chandra X-ray Observatory
Center, which is operated by the Smithsonian Astrophysical Observatory
for and on behalf of NASA. Galaxy cluster research at Harvard is
supported by NSF grant AST-1009012 and at SAO by NSF grants AST-1009649
and MRI-0723073. The McGill group acknowledges funding from the National
Sciences and Engineering Research Council of Canada, Canada Research
Chairs program, and the Canadian Institute for Advanced Research.
Argonne National Laboratory's work was supported under U.S. Department
of Energy contract DE-AC02-06CH11357. This work is based in part on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. J.E.C. acknowledges support from National Science
Foundation grants PLR-1248097 and PHY-1125897. C.R. acknowledges support
from the University of Melbourne and from the Australian Research
Councils Discovery Projects scheme (DP150103208). D.A. and T.S.
acknowledge support from the German Federal Ministry of Economics and
Technology (BMWi) provided through DLR under projects 50 OR 1210, 50 OR
1308, and 50 OR 1407.
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JI Astrophys. J.
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900003
ER
PT J
AU Steiner, JF
Walton, DJ
Garcia, JA
McClintock, JE
Laycock, SGT
Middleton, MJ
Barnard, R
Madsen, KK
AF Steiner, James F.
Walton, Dominic J.
Garcia, Javier A.
McClintock, Jeffrey E.
Laycock, Silas G. T.
Middleton, Matthew J.
Barnard, Robin
Madsen, Kristin K.
TI ON THE SPIN OF THE BLACK HOLE IN IC 10 X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; black hole physics; stars: individual (IC 10
X-1); X-rays: binaries
ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; NGC 300 X-1; NEUTRON-STAR;
ACCRETION DISK; XTE J1701-462; WOLF-RAYET; IC-10 X-1; LMC X-3;
REFLECTION SPECTROSCOPY
AB The compact X-ray source in the eclipsing X-ray binary IC 10 X-1 has reigned for years as ostensibly the most massive stellar-mass black hole, with a mass estimated to be about twice that of its closest rival. However, striking results presented recently by Laycock et al. reveal that the mass estimate, based on emission-line velocities, is unreliable and that the mass of the X-ray source is essentially unconstrained. Using Chandra and NuSTAR data, we rule against a neutron-star model and conclude that IC 10 X-1 contains a black hole. The eclipse duration of IC 10 X-1 is shorter and its depth shallower at higher energies, an effect consistent with the X-ray emission being obscured during eclipse by a Compton-thick core of a dense wind. The spectrum is strongly disk-dominated, which allows us to constrain the spin of the black hole via X-ray continuum fitting. Three other wind-fed black hole systems are known; the masses and spins of their black holes are high: M similar to 10-15M(circle dot) and a(*) > 0.8. If the mass of IC 10 X-1's black hole is comparable, then its spin is likewise high.
C1 [Steiner, James F.] MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.
[Steiner, James F.; Garcia, Javier A.; McClintock, Jeffrey E.; Barnard, Robin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Walton, Dominic J.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Laycock, Silas G. T.] Univ Massachusetts, Dept Phys, Lowell, MA 01854 USA.
[Middleton, Matthew J.] Inst Astron, Madingly Rd, Cambridge CB3 OHA, England.
[Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RP Steiner, JF (reprint author), MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.; Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Madsen, Kristin/0000-0003-1252-4891
FU Chandra [GO4-15051X]; NASA Hubble Fellowship [HST-HF-51315.01]; NASA
Einstein Fellowship [PF5-160144]; NASA
FX This research has made use of software provided by the Chandra X-ray
Center (CXC). This work was made possible by Chandra Grant GO4-15051X.
J.F.S. has been supported by the NASA Hubble Fellowship grant
HST-HF-51315.01, and the NASA Einstein Fellowship grant PF5-160144. We
thank the CXC helpdesk and Larry David for their advice on the Chandra
data reductions. J.F.S. thanks R. Remillard and J. Homan for helpful
discussions on NS spectral models. We thank the anonymous referee for
helpful criticisms which have improved this paper. This research has
made use of data obtained with the NuSTAR mission, a project led by the
California Institute of Technology (Caltech), managed by the Jet
Propulsion Laboratory (JPL) and funded by NASA, and has utilized the
NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI
Science Data Center (ASDC, Italy) and Caltech (USA). Chandra ObsId
15803.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900071
ER
PT J
AU van Weeren, RJ
Ogrean, GA
Jones, C
Forman, WR
Andrade-Santos, F
Bonafede, A
Bruggen, M
Bulbul, E
Clarke, TE
Churazov, E
David, L
Dawson, WA
Donahue, M
Goulding, A
Kraft, RP
Mason, B
Merten, J
Mroczkowski, T
Murray, SS
Nulsen, PEJ
Rosati, P
Roediger, E
Randall, SW
Sayers, J
Umetsu, K
Vikhlinin, A
Zitrin, A
AF van Weeren, R. J.
Ogrean, G. A.
Jones, C.
Forman, W. R.
Andrade-Santos, F.
Bonafede, A.
Brueggen, M.
Bulbul, E.
Clarke, T. E.
Churazov, E.
David, L.
Dawson, W. A.
Donahue, M.
Goulding, A.
Kraft, R. P.
Mason, B.
Merten, J.
Mroczkowski, T.
Murray, S. S.
Nulsen, P. E. J.
Rosati, P.
Roediger, E.
Randall, S. W.
Sayers, J.
Umetsu, K.
Vikhlinin, A.
Zitrin, A.
TI THE DISCOVERY OF LENSED RADIO AND X-RAY SOURCES BEHIND THE FRONTIER
FIELDS CLUSTER MACS J0717.5+3745 WITH THE JVLA AND CHANDRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (MACS J0717.5+3745); gravitational
lensing: strong; radio continuum: galaxies
ID ACTIVE GALACTIC NUCLEI; MERGER ABELL 2744; GALAXY CLUSTERS;
STAR-FORMATION; PARAMETER-ESTIMATION; MASS RECONSTRUCTION; LUMINOSITY
FUNCTION; MAGNIFICATION MAPS; NUMBER COUNTS; W-PROJECTION
AB We report on high-resolution JVLA and Chandra observations of the Hubble Space Telescope (HST) Frontier Cluster MACS J0717.5+3745. MACS J0717.5+3745 offers the largest contiguous magnified area of any known cluster, making it a promising target to search for lensed radio and X-ray sources. With the high-resolution 1.0-6.5 GHz JVLA imaging in A and B configuration, we detect a total of 51 compact radio sources within the area covered by the HST imaging. Within this sample, we find seven. lensed sources with amplification factors larger than two. None of these sources are identified as multiply lensed. Based on the radio luminosities, the majority of these sources are likely star-forming galaxies with star-formation rates (SFRs) of 10-50 M-circle dot yr(-1) located at 1 less than or similar to z less than or similar to 2. Two of the lensed radio sources are also detected in the Chandra image of the cluster. These two sources are likely active galactic nuclei, given their 2-10 keV X-ray luminosities of similar to 10(43-44) erg s(-1). From the derived radio luminosity function, we find evidence for an increase in the number density of radio sources at 0.6 < z < 2.0, compared to a z < 0.3 sample. Our observations indicate that deep radio imaging of lensing clusters can be used to study star-forming galaxies, with SFRs as low as similar to 10(circle dot) yr(-1), at the peak of cosmic star formation history.
C1 [van Weeren, R. J.; Ogrean, G. A.; Jones, C.; Forman, W. R.; Andrade-Santos, F.; Bulbul, E.; David, L.; Kraft, R. P.; Murray, S. S.; Nulsen, P. E. J.; Randall, S. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bonafede, A.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Clarke, T. E.; Mroczkowski, T.] US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Churazov, E.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Churazov, E.] Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Dawson, W. A.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Goulding, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Mason, B.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Merten, J.] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA.
[Nulsen, P. E. J.] Univ Western Australia, ICRAR, 35 Stirling Hwy, Crawley, WA 6009, Australia.
[Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy.
[Roediger, E.] Univ Hull, EA Milne Ctr Astrophys, Dept Math & Phys, Cottinton Rd, Kingston Upon Hull HU6 7RX, N Humberside, England.
[Sayers, J.; Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, MC 249-17, Pasadena, CA 91125 USA.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rvanweeren@cfa.harvard.edu
RI Churazov, Eugene/A-7783-2013;
OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu,
Keiichi/0000-0002-7196-4822; Nulsen, Paul/0000-0003-0297-4493; van
Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682
FU National Aeronautics and Space Administration through Chandra Award
[GO4-15129X]; National Aeronautics Space Administration [NAS8-03060];
NASA through the Einstein Postdoctoral grant - Chandra X-ray Center
[PF2-130104]; NASA [NAS8-03060, NAS5-26555]; NASA through a Hubble
Fellowship - Space Telescope Science Institute [HST-HF2-51345.001-A];
Deutsche Forschungsgemeinschaft [FOR 1254]; Smithsonian Institution;
Chandra grant [GO3-14131X]; NASA through Hubble Fellowship - STScI
[HST-HF2-51334.001-A]; 6.1 Base funding; STScI grant [12065.007-A]; U.S.
DOE [DE-AC52-07NA27344]
FX We thank the anonymous referee for useful comments. We thank Megan
Gralla for a discussion on the lensed radio sources. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number GO4-15129X issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
Space Administration under contract NAS8-03060. R.J.W. is supported by
NASA through the Einstein Postdoctoral grant number PF2-130104 awarded
by the Chandra X-ray Center, which is operated by the Smithsonian
Astrophysical Observatory for NASA under contract NAS8-03060. G.A.O.
acknowledges support by NASA through a Hubble Fellowship grant
HST-HF2-51345.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555. M.B.
acknowledges support by the research group FOR 1254 funded by the
Deutsche Forschungsgemeinschaft: "Magnetization of interstellar and
intergalactic media: the prospects of low-frequency radio observations."
W.R.F., C.J., and F.A.-S. acknowledge support from the Smithsonian
Institution. F.A.-S. acknowledges support from Chandra grant GO3-14131X.
A.Z. is supported by NASA through Hubble Fellowship grant
HST-HF2-51334.001-A awarded by STScI. This research was performed while
T.M. held a National Research Council Research Associateship Award at
the Naval Research Laboratory (NRL). Basic research in radio astronomy
at NRL by T.M. and T.E.C. is supported by 6.1 Base funding. M.D.
acknowledges the support of STScI grant 12065.007-A. P.E.J.N. was
partially supported by NASA contract NAS8-03060. E.R. acknowledges a
Visiting Scientist Fellowship of the Smithsonian Astrophysical
Observatory, and the hospitality of the Center for Astrophysics in
Cambridge. Part of this work performed under the auspices of the U.S.
DOE by LLNL under Contract DE-AC52-07NA27344.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900015
ER
PT J
AU Zhao, JH
Morris, MR
Goss, WM
AF Zhao, Jun-Hui
Morris, Mark R.
Goss, W. M.
TI A NEW PERSPECTIVE OF THE RADIO BRIGHT ZONE AT THE GALACTIC CENTER:
FEEDBACK FROM NUCLEAR ACTIVITIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; H II regions; ISM: individual objects (Sagittarius A);
ISM: jets and outflows; ISM: supernova remnants; radio continuum: ISM
ID SAGITTARIUS-A-ASTERISK; HIGH-RESOLUTION OBSERVATIONS; PASCHEN-ALPHA
SURVEY; MASSIVE BLACK-HOLE; SGR-A; SUPERNOVA REMNANT; CENTER REGION;
IONIZED-GAS; CENTRAL PARSEC; MILKY-WAY
AB New observations of Sgr A have been carried out with the Jansky VLA in the B and C arrays using the broadband (2 GHz) continuum mode at 5.5 GHz. The field of view covers the central 13' (30 pc) region of the radio-bright zone at the Galactic center. Using the multi-scale and multi-frequency-synthesis (MS-MFS) algorithms in CASA, we have imaged Sgr A with a resolution of 1 '', achieving an rms noise of 8 mu Jy beam(-1), and a dynamic range of 100,000:1. Both previously known and newly identified radio features in this region are revealed, including numerous filamentary sources. The radio continuum image is compared with Chandra X-ray images, with a CN emission-line image obtained with the Submillimeter Array and with detailed Paschen-alpha images obtained with Hubble Space Telescope/NICMOS. We discuss several prominent features in the radio image. The "Sgr A west Wings" extend 2' (5 pc) from the NW and SE tips of the Sgr A west H II region (the "Mini-spiral") to positions located 2.9 and 2.4 arcmin to the northwest and southeast of Sgr A*, respectively. The NW wing, along with several other prominent features, including the previously identified "NW Streamers," form an elongated radio lobe (NW lobe), oriented nearly perpendicular to the Galactic plane. This radio lobe, with a size of 6.'3 x 3.'2 (14.4 pc x 7.3 pc), has a known X-ray counterpart. In the outer region of the NW lobe, a row of three thermally emitting rings is observed. A field containing numerous amorphous radio blobs extends for a distance of similar to 2 arcmin beyond the tip of the SE wing; these newly recognized features coincide with the SE X-ray lobe. Most of the amorphous radio blobs in the NW and SE lobes have Paschen-alpha counterparts. We propose that they have been produced by shock interaction of ambient gas concentrations with a collimated nuclear wind or an outflow that originated from within the circumnuclear disk (CND). We also discuss the possibility that the ionized wind or outflow has been launched by radiation force produced by the central star cluster. Finally, we remark on the detailed structure of a prominent radio emission feature located within the shell of the Sgr A east supernova remnant. Because this feature-the "Sigma Front"-correlates well in shape and orientation with the nearby edge of the CND, we propose that it is a reflected shock wave resulting from the impact of the Sgr A east blast wave on the CND.
C1 [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Morris, Mark R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Goss, W. M.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jzhao@cfa.harvard.edu
OI Morris, Mark/0000-0002-6753-2066
NR 91
TC 1
Z9 1
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2016
VL 817
IS 2
AR 171
DI 10.3847/0004-637X/817/2/171
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7YU
UT WOS:000369437900088
ER
PT J
AU Kimball, BA
Stelting, SA
McAuliffe, TW
Stahl, RS
Garcia, RA
Pitt, WC
AF Kimball, Bruce A.
Stelting, Scott A.
McAuliffe, Thomas W.
Stahl, Randal S.
Garcia, Rafael A.
Pitt, William C.
TI Development of artificial bait for brown treesnake suppression
SO BIOLOGICAL INVASIONS
LA English
DT Article
DE Boiga irregularis; Interdiction; Invasive; Pacific islands; Vertebrate
ID GARTER SNAKES; SIGNAL-TRANSDUCTION; VOMERONASAL SYSTEM;
RECEPTOR-BINDING; ISLAND; CHEMOATTRACTANT; AVERSION; GUAM
AB The brown treesnake (Boiga irregularis) was accidentally introduced to Guam in the 1940s from the Admiralty Islands. A native of Australia, Papua New Guinea, and the Solomon Islands, the brown treesnake (BTS) continues to threaten the economy and ecology of Guam and is currently the subject of a cooperative program to control snake populations on the island and prevent its spread throughout the Pacific Rim. Delivery of toxic baits is a primary component of population suppression efforts. While many food items tested as baits for toxicant delivery provide relevant food prey cues leading to investigatory behaviors in BTS, only a few items tested in the past two decades have adequately promoted reliable consumption. Chief among them is the dead neonatal mouse (DNM). A series of chemical and bioassays were performed to identify materials with similar sensory qualities as DNM. Among the many items tested in a series of field experiments with free-ranging BTS in Guam, a processed meat product treated with an artificial mouse fat mixture was found to be removed from bait stations at rates greater than previously tested DNM substitutes and approaching removal rates of DNM. Furthermore, the test baits demonstrated excellent durability under field conditions. Further development of this bait offers great potential to satisfy many desirable attributes for BTS baiting operations.
C1 [Kimball, Bruce A.] Anim & Plant Hlth Inspect Serv, USDA, Wildlife Serv, Natl Wildlife Res Ctr,Monell Chem Senses Ctr, Philadelphia, PA 19104 USA.
[Stelting, Scott A.; Stahl, Randal S.] Anim & Plant Hlth Inspect Serv, USDA, Wildlife Serv, Natl Wildlife Res Ctr, Ft Collins, CO 80521 USA.
[McAuliffe, Thomas W.] Anim & Plant Hlth Inspect Serv, USDA, Wildlife Serv, Natl Wildlife Res Ctr, Hilo, HI 96720 USA.
[Garcia, Rafael A.] ARS, USDA, Eastern Reg Res Ctr, Biobased & Other Anim Coprod Res Unit, Wyndmoor, PA 19038 USA.
[Pitt, William C.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
RP Kimball, BA (reprint author), Anim & Plant Hlth Inspect Serv, USDA, Wildlife Serv, Natl Wildlife Res Ctr,Monell Chem Senses Ctr, 3500 Market St, Philadelphia, PA 19104 USA.
EM bruce.a.kimball@aphis.usda.gov
FU U.S. Department of Interior Office of Insular Affairs [101580RU033];
U.S. Department of the Navy (MIPR) [N6274212MP00024]
FX These studies were made possible through funding provided by the U.S.
Department of Interior Office of Insular Affairs (Agreement 101580RU033)
and U.S. Department of the Navy (MIPR# N6274212MP00024) and generous
access to Andersen AFB. The assistance of USDA-APHIS-WS staff located on
the island of Guam was greatly appreciated; especially Daniel S. Vice
(1970-2014), Assistant State Director for the Hawaii/Guam Program, who
dedicated much of his career to the control and interdiction of invasive
species. Spam (R) is a registered trademark of Hormel Food Corporation
(Austin, MN). ARASCO (R) is a registered trademark of DSM Nutritional
Products (Columbia, MD). We thank DSM Nutritional Products for providing
a complimentary sample of ARASCO (R). Mention of specific trade names
does not constitute endorsement by the US Department of Agriculture.
NR 20
TC 0
Z9 0
U1 9
U2 16
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1387-3547
EI 1573-1464
J9 BIOL INVASIONS
JI Biol. Invasions
PD FEB
PY 2016
VL 18
IS 2
BP 359
EP 369
DI 10.1007/s10530-015-1031-z
PG 11
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DD6WV
UT WOS:000370066200005
ER
PT J
AU Turner, BC
de Rivera, CE
Grosholz, ED
Ruiz, GM
AF Turner, B. C.
de Rivera, C. E.
Grosholz, E. D.
Ruiz, G. M.
TI Assessing population increase as a possible outcome to management of
invasive species
SO BIOLOGICAL INVASIONS
LA English
DT Article
DE Carcinus maenas; European green crab; Hydra effect; Management of
invasion; Overcompensation
ID TILAPIA OREOCHROMIS-MOSSAMBICUS; PREDATOR-PREY INTERACTIONS; BASS
MICROPTERUS-DOLOMIEU; STAGE-SPECIFIC BIOMASS; CRABS CARCINUS-MAENAS;
EUROPEAN GREEN CRAB; JUVENILE BLUE-CRAB; GROWTH-RATE; DYNAMICS;
MORTALITY
AB Some efforts to reduce invasive populations have paradoxically led to population increases. This phenomenon, referred to as overcompensation, occurs when reduced intraspecific pressures increase juvenile survival or maturation rates, leading to increased population size. Overcompensation in response to eradication efforts could derail management efforts, so it would be beneficial to evaluate the likelihood of overcompensation prior to removal. We conducted a series of experiments to examine the potential for overcompensation of a non-native population of the European green crab, Carcinus maenas, which was being removed in Bodega Harbor, California. First, we examined the impact of adults on juvenile survival by measuring adult cannibalism on juveniles in the presence and absence of alternative prey, and the survival of tethered juveniles at varying adult densities. Second, we examined how adult presence affected juvenile short-term foraging and growth rates. Although adult presence reduced juvenile short-term foraging, we detected only minimal cannibalism and found no evidence that adults greatly reduce juvenile growth or survivorship. These results suggest that overcompensation is not likely to occur in this population in response to removal. We assessed this prediction using pre- and post-removal surveys of juvenile recruitment in Bodega Harbor compared to nearby populations, testing for evidence of overcompensation. Relative juvenile abundance did not statistically increase in removal compared to reference populations, consistent with our conclusion from the experiments. This experimental approach which focuses on an organism's population biology provides a tool to assess capacity for assessing the capacity for overcompensation in management strategies for invasive species.
C1 [Turner, B. C.; de Rivera, C. E.; Ruiz, G. M.] Portland State Univ, Dept Environm Sci & Management, Portland, OR 97201 USA.
[Grosholz, E. D.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA.
[Ruiz, G. M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Turner, BC (reprint author), Portland State Univ, Dept Environm Sci & Management, Portland, OR 97201 USA.
EM bcturner@pdx.edu
OI Ruiz, Gregory/0000-0003-2499-441X
FU NSF GK12 [0948041]; Pacific Marine Fisheries Commission; NOAA
[NA06OAR4170261, NA06OAR4170159, NA07OAR4170501, NA08OAR4170927]; Alaska
Department of Fish and Game [IHP-07-146]
FX For their help collecting data, we would like to thank: B. Kordas, A.
Larson, C. Coleman-Hulbert, S. Attoe, I. Clarke, R. Jeppesen, B. Cheng,
D. Kimbro, A. Bakus, A. Deck, S. Koetke, C. Brown, G. Ashton, A. Newsom,
B. Marshman, B. Powell, C. Kucey and G. Turner. We would also like to
thank C. Parker and B. Steves for their invaluable statistical
assistance. Financial support was provided (in part) by the, NSF GK12 (#
0948041) in support of BCT, and by Pacific Marine Fisheries Commission
and NOAA (## NA06OAR4170261, NA06OAR4170159, NA07OAR4170501,
NA08OAR4170927), and Alaska Department of Fish and Game (# IHP-07-146).
NR 58
TC 1
Z9 1
U1 15
U2 35
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1387-3547
EI 1573-1464
J9 BIOL INVASIONS
JI Biol. Invasions
PD FEB
PY 2016
VL 18
IS 2
BP 533
EP 548
DI 10.1007/s10530-015-1026-9
PG 16
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DD6WV
UT WOS:000370066200019
ER
PT J
AU Mcelroy, MT
AF Mcelroy, Matthew T.
TI Teasing apart crypsis and aposematism - evidence that disruptive
coloration reduces predation on a noxious toad
SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE aposematic; background matching; Barro Colorado Island; Bufo typhonius;
camouflage; cryptic coloration; predation; predator; prey; Rhinella
margaritifera
ID RANGING AVIAN PREDATORS; POISON FROG; CORRELATIONAL SELECTION;
ANTIPREDATOR BEHAVIOR; THAMNOPHIS-ORDINOIDES; GARTER SNAKE; PATTERN;
PREY; AVOIDANCE; DEFENSE
AB Both cryptic and aposematic colour patterns can reduce predation risk to prey. These distinct strategies may not be mutually exclusive, because the impact of prey coloration depends on a predator's sensory system and cognition and on the environmental background. Determining whether prey signals are cryptic or aposematic is a prerequisite for understanding the ecological and evolutionary implications of predator-prey interactions. This study investigates whether coloration and pattern in an exceptionally polymorphic toad, Rhinella alata, from Barro Colorado Island, Panama reduces predation via background matching, disruptive coloration, and/or aposematic signaling. When clay model replicas of R. alata were placed on leaf litter, the model's dorsal pattern but not its colour - affected attack rates by birds. When models were placed on white paper, patterned and un-patterned replicas had similar attack rates by birds. These results indicate that dorsal patterns in R. alata are functionally cryptic and emphasize the potential effectiveness of disruptive coloration in a vertebrate taxon. (C) 2015 The Linnean Society of London
C1 [Mcelroy, Matthew T.] Univ Washington, Dept Biol, Seattle, WA 98195 USA.
[Mcelroy, Matthew T.] Univ Washington, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA.
[Mcelroy, Matthew T.] Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama.
RP Mcelroy, MT (reprint author), Univ Washington, Dept Biol, Seattle, WA 98195 USA.; Mcelroy, MT (reprint author), Univ Washington, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA.; Mcelroy, MT (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama.
EM mtm3@uw.edu
FU STRI 'A. Stanley Rand' Fellowship
FX I thank J. Christy and R. Sapporito for experimental advice; O. Acevido
and BCI/STRI Staff for logistical support; BCI game wardens for
transportation; and H. Rogers, R. Huey, the A. Leache Lab, and three
anonymous reviewers for improvements to the manuscript. Funding was
provided by the STRI 'A. Stanley Rand' Fellowship.
NR 49
TC 1
Z9 1
U1 14
U2 32
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4066
EI 1095-8312
J9 BIOL J LINN SOC
JI Biol. J. Linnean Soc.
PD FEB
PY 2016
VL 117
IS 2
BP 285
EP 294
DI 10.1111/bij.12669
PG 10
WC Evolutionary Biology
SC Evolutionary Biology
GA DD8ET
UT WOS:000370158900009
ER
PT J
AU Pyenson, ND
Parham, JF
Velez-Juarbe, J
AF Pyenson, Nicholas D.
Parham, James F.
Velez-Juarbe, Jorge
TI The dilemma of trade samples and the importance of museum
vouchers-caveats from a study on the extinction of Steller's sea cow: a
comment on Crerar et al. (2014)
SO BIOLOGY LETTERS
LA English
DT Letter
C1 [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
[Parham, James F.; Velez-Juarbe, Jorge] Calif State Univ Fullerton, John D Cooper Archaeol & Paleontol Ctr, Dept Geol Sci, Fullerton, CA 92834 USA.
[Velez-Juarbe, Jorge] Nat Hist Museum Los Angeles Cty, Dept Mammal, Los Angeles, CA 90007 USA.
RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
EM pyensonn@si.edu
NR 5
TC 1
Z9 1
U1 0
U2 4
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1744-9561
EI 1744-957X
J9 BIOL LETTERS
JI Biol. Lett.
PD FEB 1
PY 2016
VL 12
IS 2
AR 20150149
DI 10.1098/rsbl.2015.0149
PG 2
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DD5PU
UT WOS:000369977200001
PM 26843552
ER
PT J
AU Fahey, C
Winter, K
Slot, M
Kitajima, K
AF Fahey, Catherine
Winter, Klaus
Slot, Martijn
Kitajima, Kaoru
TI Influence of arbuscular mycorrhizal colonization on whole-plant
respiration and thermal acclimation of tropical tree seedlings
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Acclimation; carbon; climate; Panama; phosphorus; symbiosis
ID LEAF RESPIRATION; TEMPERATURE SENSITIVITY; ELEVATED-TEMPERATURES; FOLIAR
RESPIRATION; ROOT RESPIRATION; CARBON BALANCE; HOST-PLANT; GROWTH;
FOREST; RESPONSES
AB Symbiotic arbuscular mycorrhizal fungi (AMF) are ubiquitous in tropical forests. AMF play a role in the forest carbon cycle because they can increase nutrient acquisition and biomass of host plants, but also incur a carbon cost to the plant. Through their interactions with their host plants they have the potential to affect how plants respond to environmental perturbation such as global warming. Our objective was to experimentally determine how plant respiration rates and responses to warmer environment are affected by AMF colonization in seedlings of five tropical tree species at the whole plant level. We evaluated the interaction between AMF colonization and temperature on plant respiration against four possible outcomes; acclimation does or does not occur regardless of AMF, or AMF can increase or decrease respiratory acclimation. Seedlings were inoculated with AMF spores or sterilized inoculum and grown at ambient or elevated nighttime temperature. We measured whole plant and belowground respiration rates, as well as plant growth and biomass allocation. There was an overall increase in whole plant, root, and shoot respiration rate with AMF colonization, whereas temperature acclimation varied among species, showing support for three of the four possible responses. The influence of AMF colonization on growth and allocation also varied among plant species. This study shows that the effect of AMF colonization on acclimation differs among plant species. Given the cosmopolitan nature of AMF and the importance of plant acclimation for predicting climate feedbacks a better understanding of the patterns and mechanisms of acclimation is essential for improving predictions of how climate warming may influence vegetation feedbacks.
C1 [Fahey, Catherine; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Winter, Klaus; Slot, Martijn; Kitajima, Kaoru] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Kitajima, Kaoru] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan.
RP Fahey, C (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
EM cfahey@ufl.edu
FU Smithsonian Tropical Research Institute Short-term Fellowship; NSF-IOS
[1051789]
FX This project was supported by a Smithsonian Tropical Research Institute
Short-term Fellowship (CF) and NSF-IOS grant 1051789 (KK).
NR 46
TC 3
Z9 3
U1 3
U2 24
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD FEB
PY 2016
VL 6
IS 3
BP 859
EP 870
DI 10.1002/ece3.1952
PG 12
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA DD5OY
UT WOS:000369974900020
PM 26865973
ER
PT J
AU Pinto, CM
Soto-Centeno, JA
Quiroz, AMN
Ferreyra, N
Delgado-Espinoza, F
Stahl, PW
Tirira, DG
AF Pinto, C. Miguel
Soto-Centeno, J. Angel
Quiroz, Angela M. Nunez
Ferreyra, Nicolas
Delgado-Espinoza, Florencio
Stahl, Peter W.
Tirira, Diego G.
TI Archaeology, biogeography, and mammalogy do not provide evidence for
tarukas (Cervidae: Hippocamelus antisensis) in Ecuador
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE Agua Blanca; Andes; Cervidae; distribution records; Ecuador; Huancabamba
depression; Manteno; South America; taruka; zooarchaeology
ID SPECIES DISTRIBUTION MODELS; LAST GLACIAL MAXIMUM; GEOGRAPHIC
DISTRIBUTIONS; WESTERN ECUADOR; DIVERSITY; ANDES; DEER; CONSERVATION;
BIODIVERSITY; ACCURACY
AB Knowing whether a species has been extirpated, or if it ever inhabited a specific geographic area, has direct importance for planning conservation activities. The taruka (Hippocamelus antisensis) is one of the largest Neotropical mammals; it is distributed in the central Andes, and there are published records of this species in Ecuador. Recently, missing museum specimens have cast doubts on the validity of these Ecuadorian records. Here, we examine whether the taruka ever inhabited Ecuador by analyzing multiple sources of information. Our approach consists of 3 components: 1) we surveyed archaeological collections and literature for any biological remains and cultural artifacts that may represent tarukas, 2) we searched mammal collections for specimens reported in publications, and 3) we generated ecological niche models (ENMs) of current and past climates to determine whether Ecuador offers suitable habitats for the taruka. Our results suggest that the taruka never inhabited Ecuador. We did not find any reliable supporting evidence in the form of specimens nor convincing literature reports. Furthermore, ENMs revealed that Ecuador has not supported suitable climates for the taruka. We suggest that published records of taruka in Ecuador may have been due to improper identifications of specimens. The methods used here may also prove useful in determining the presence of species that are either thought to be extinct, or suspected to be recently introduced into a new geographic area.
C1 [Pinto, C. Miguel] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, 1000 Constitution Ave, Washington, DC 20560 USA.
[Pinto, C. Miguel; Soto-Centeno, J. Angel] Amer Museum Nat Hist, Dept Mammal, Cent Pk West 79th St, New York, NY 10024 USA.
[Pinto, C. Miguel; Soto-Centeno, J. Angel] Amer Museum Nat Hist, Sackler Inst Comparat Gen, Cent Pk West 79th St, New York, NY 10024 USA.
[Pinto, C. Miguel] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Cetr Invest Enfermedades Infecciosas & Cronicas, Av 12 Octubre & Carr, Quito 17012184, Ecuador.
[Quiroz, Angela M. Nunez] Ministerio Medio Ambiente & Agua, Direcc Gen Biodiversidad & Areas Protegidas, Av 20 Octubre & Capitan Castrillo 434, La Paz, Bolivia.
[Ferreyra, Nicolas] Fdn Bioandina Argentina, Republ India 3000, RA-1425 Buenos Aires, DF, Argentina.
[Ferreyra, Nicolas] Adm Parques Nacl, Parque Nacl Lanin, Emilio Frey 749, RA-8370 San Martin, Argentina.
[Delgado-Espinoza, Florencio] Univ San Francisco, Colegio Artes Liber, Diego Robles & Via Interocean, Quito 171200841, Ecuador.
[Stahl, Peter W.] Univ Victoria, Dept Anthropol, 3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
[Tirira, Diego G.] Pontificia Univ Catol Ecuador, Escuela Ciencias Biol, Museo Zool, Av 12 Octubre & Carr, Quito 17012184, Ecuador.
[Tirira, Diego G.] Fdn Mamiferos & Conservac, Victor Balseca 100 & Gen Gribaldo Mino, Conocoto 17012184, Quito, Ecuador.
RP Pinto, CM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, 1000 Constitution Ave, Washington, DC 20560 USA.; Pinto, CM (reprint author), Amer Museum Nat Hist, Dept Mammal, Cent Pk West 79th St, New York, NY 10024 USA.; Pinto, CM (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Gen, Cent Pk West 79th St, New York, NY 10024 USA.; Pinto, CM (reprint author), Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Cetr Invest Enfermedades Infecciosas & Cronicas, Av 12 Octubre & Carr, Quito 17012184, Ecuador.
EM pintom@si.edu
FU Fundacion Mamiferos y Conservacion; FMNH; AMNH
FX We thank B. D. Patterson and B. Stanley (Field Museum of Natural History
[FMNH]), David Flores and Olga Vaccaro (Museo Argentino de Ciencias
Naturales [MACN]), Estelina Quinatoa (Museo del Banco Central del
Ecuador [MBCE]), and Josefina Barreiro (Museo Nacional de Ciencias
Naturales [MNCN]) for their comments on the specimens under their care
and for assistance during our visits to their collections: DGT (MNCN,
MACN) and CMP (FMNH, MBCE). CMP thanks M. Soley-Guardia, P. A.
Menendez-Guerrero, and R. A. Boria for initial discussions on modeling
analyses. J. Barrio provided insightful discussions on Hippocamelus. P.
Jarrin-V. generously photographed the piece in Figure 1 and A. Grosset
kindly permitted us to use his photograph of H. antisensis. A. Sexenian
(Museo de Historia Natural de Montevideo) and R. S. Voss (American
Museum of Natural History [AMNH]) provided literature. We are thankful
to all participating institutions in MaNIS and SBI portals for providing
locality data. Funding to visit museums was provided by Fundacion
Mamiferos y Conservacion to DGT and a FMNH Visiting Scholarship to CMP.
Funding for JAS-C was provided by Theodore Roosevelt and Gerstner
Scholar postdoctoral fellowships at AMNH. We thank L. Shipley and E.
Yensen whose valuable comments greatly enhanced the quality of this
contribution.
NR 99
TC 0
Z9 0
U1 1
U2 3
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD FEB
PY 2016
VL 97
IS 1
BP 41
EP 53
DI 10.1093/jmammal/gyv151
PG 13
WC Zoology
SC Zoology
GA DC5AP
UT WOS:000369232600005
ER
PT J
AU Huang, CH
Sun, RR
Hu, Y
Zeng, LP
Zhang, N
Cai, LM
Zhang, Q
Koch, MA
Al-Shehbaz, I
Edger, PP
Pires, JC
Tan, DY
Zhong, Y
Ma, H
AF Huang, Chien-Hsun
Sun, Renran
Hu, Yi
Zeng, Liping
Zhang, Ning
Cai, Liming
Zhang, Qiang
Koch, Marcus A.
Al-Shehbaz, Ihsan
Edger, Patrick P.
Pires, J. Chris
Tan, Dun-Yan
Zhong, Yang
Ma, Hong
TI Resolution of Brassicaceae Phylogeny Using Nuclear Genes Uncovers Nested
Radiations and Supports Convergent Morphological Evolution
SO MOLECULAR BIOLOGY AND EVOLUTION
LA English
DT Article
DE ancestral character reconstruction; Brassicaceae; divergence time
estimation; orthologous nuclear gene; phylogeny; transcriptome
ID ARABIDOPSIS-THALIANA; MOLECULAR EVOLUTION; SPECIES RADIATION; DIVERGENCE
TIMES; L. BRASSICACEAE; SEQUENCE ALIGNMENT; ABSOLUTE RATES; CHS
SEQUENCES; MIXED MODELS; PLANT
AB Brassicaceae is one of the most diverse and economically valuable angiosperm families with widely cultivated vegetable crops and scientifically important model plants, such as Arabidopsis thaliana. The evolutionary history, ecological, morphological, and genetic diversity, and abundant resources and knowledge of Brassicaceae make it an excellent model family for evolutionary studies. Recent phylogenetic analyses of the family revealed three major lineages (I, II, and III), but relationships among and within these lineages remain largely unclear. Here, we present a highly supported phylogeny with six major clades using nuclear markers from newly sequenced transcriptomes of 32 Brassicaceae species and large data sets from additional taxa for a total of 55 species spanning 29 out of 51 tribes. Clade A consisting of Lineage I and Macropodium nivale is sister to combined Clade B (with Lineage II and others) and a new Clade C. The ABC clade is sister to Clade D with species previously weakly associated with Lineage II and Clade E (Lineage III) is sister to the ABCD clade. Clade F (the tribe Aethionemeae) is sister to the remainder of the entire family. Molecular clock estimation reveals an early radiation of major clades near or shortly after the Eocene-Oligocene boundary and subsequent nested divergences of several tribes of the previously polytomous Expanded Lineage II. Reconstruction of ancestral morphological states during the Brassicaceae evolution indicates prevalent parallel (convergent) evolution of several traits over deep times across the entire family. These results form a foundation for future evolutionary analyses of structures and functions across Brassicaceae.
C1 [Huang, Chien-Hsun; Sun, Renran; Zeng, Liping; Cai, Liming; Zhong, Yang; Ma, Hong] Fudan Univ, Sch Life Sci, State Key Lab Genet Engn, Shanghai 200433, Peoples R China.
[Huang, Chien-Hsun; Sun, Renran; Zeng, Liping; Cai, Liming; Zhong, Yang; Ma, Hong] Fudan Univ, Key Lab Biodivers Sci & Ecol Engn, Collaborat Innovat Ctr Genet & Dev,Sch Life Sci,M, Inst Plant Biol,Inst Biodivers Sci,Ctr Evolutiona, Shanghai 200433, Peoples R China.
[Hu, Yi] Penn State Univ, Huck Inst Life Sci, Dept Biol, University Pk, PA 16802 USA.
[Zhang, Ning] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20560 USA.
[Zhang, Qiang] Guangxi Zhuang Autonomous Region & Chinese Acad S, Guangxi Inst Bot, Guangxi Key Lab Plant Conservat & Restorat Ecol K, Guilin, Peoples R China.
[Koch, Marcus A.] Heidelberg Univ, Ctr Organismal Studies Heidelberg, Biodivers & Plant Systemat, Heidelberg, Germany.
[Al-Shehbaz, Ihsan] Missouri Bot Garden, St Louis, MO USA.
[Edger, Patrick P.] Michigan State Univ, Dept Hort, E Lansing, MI 48824 USA.
[Pires, J. Chris] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA.
[Tan, Dun-Yan] Xinjiang Agr Univ, Xinjiang Key Lab Grassland Resources & Ecol, Coll Grassland & Environm Sci, Urumqi, Peoples R China.
RP Ma, H (reprint author), Fudan Univ, Sch Life Sci, State Key Lab Genet Engn, Shanghai 200433, Peoples R China.
EM hongma@fudan.edu.cn
RI Koch, Marcus/A-4924-2011; Huang, Chien-Hsun/E-1609-2016
OI Koch, Marcus/0000-0002-1693-6829;
FU National Natural Science Foundation of China [91131007]; China
Postdoctoral Science Foundation [2014M551316]; State Key Laboratory of
Genetic Engineering at Fudan University; USA National Science Foundation
[DEB 1146603]; NSF [NSF-NPGI 1202793]; German Research Foundation [DFG
2302-13/1]
FX We thank Dr Wenju Zhang (Fudan University) for the assistance in
material collection, Dr Fan Lu (Fudan University) and Dr Guiling Zhou
(Xinjiang Agricultural University) for specimen identification. We also
thank Dr Ji Qi (Fudan University) for help in transcriptome sequence
assembly. This work was supported by grants from the National Natural
Science Foundation of China (grant number 91131007); the China
Postdoctoral Science Foundation (grant number 2014M551316); funds from
the State Key Laboratory of Genetic Engineering at Fudan University; USA
National Science Foundation grant (DEB 1146603 to J.C.P.); NSF Plant
Genome postdoctoral grant (NSF-NPGI 1202793 to P.P.E.); and German
Research Foundation (DFG 2302-13/1 to M.A.K.).
NR 121
TC 16
Z9 19
U1 19
U2 56
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0737-4038
EI 1537-1719
J9 MOL BIOL EVOL
JI Mol. Biol. Evol.
PD FEB
PY 2016
VL 33
IS 2
BP 394
EP 412
DI 10.1093/molbev/msv226
PG 19
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA DD5VU
UT WOS:000369993600010
PM 26516094
ER
PT J
AU Valenzuela-Toro, AM
Pyenson, ND
Gutstein, CS
Suarez, ME
AF Valenzuela-Toro, Ana M.
Pyenson, Nicholas D.
Gutstein, Carolina S.
Suarez, Mario E.
TI A NEW DWARF SEAL FROM THE LATE NEOGENE OF SOUTH AMERICA AND THE
EVOLUTION OF PINNIPEDS IN THE SOUTHERN HEMISPHERE
SO PAPERS IN PALAEONTOLOGY
LA English
DT Article
DE Phocidae; late Miocene; Chile; Peru; South Pacific Ocean
ID NORTH-CENTRAL CHILE; TROPICAL EASTERN PACIFIC; CARNIVORA OTARIIDAE;
MAMMALIA CARNIVORA; FOSSIL SEABIRDS; LATE MIOCENE; TRUE SEALS;
BODY-SIZE; PHYLOGENY; PERU
AB Along the south-western coast of South America, three genera of fossil phocids (true seals) have been formally described from the late Neogene: Acrophoca and Piscophoca from Chile and Peru, and, more recently, Hadrokirus from Peru, which all represent medium-to large-sized phocids. Here, we report the discovery of Australophoca changorum gen. et sp. nov., a diminutive phocid from the late Miocene of the Bahia Inglesa Formation (northern Chile) and Pisco Formation (southern Peru), comparable in size with the smallest species of modern phocids. This taxon is based on diagnostic postcranial material, including a humerus that has an elongated deltopectoral crest but lacks an entepicondylar foramen; a femur with a subtrochanteric fossa, among other characters; in combination with a relatively small body size. All these features together distinguish A. changorum from all other reported pinnipeds. This new taxon not only increases the taxonomic and morphological diversity of phocids of the late Neogene of the eastern South Pacific Ocean, but it also provides new insights about the evolutionary history of fossil pinniped assemblages in South America and, broadly, in the southern hemisphere.
C1 [Valenzuela-Toro, Ana M.; Gutstein, Carolina S.; Suarez, Mario E.] Univ Chile, Red Paleontol, Lab Ontogenia & Filogenia, Dept Biol,Fac Ciencias, Las Palmeras 3425, Santiago, Chile.
[Valenzuela-Toro, Ana M.; Pyenson, Nicholas D.; Gutstein, Carolina S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
[Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA.
[Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA.
[Gutstein, Carolina S.] Consejo Monumentos Nacl, Area Patrimonio Nat, Vicuna Mackenna 84, Santiago, Chile.
RP Valenzuela-Toro, AM; Gutstein, CS; Suarez, ME (reprint author), Univ Chile, Red Paleontol, Lab Ontogenia & Filogenia, Dept Biol,Fac Ciencias, Las Palmeras 3425, Santiago, Chile.; Valenzuela-Toro, AM; Pyenson, ND; Gutstein, CS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.; Pyenson, ND (reprint author), Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA.; Pyenson, ND (reprint author), Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA.; Gutstein, CS (reprint author), Consejo Monumentos Nacl, Area Patrimonio Nat, Vicuna Mackenna 84, Santiago, Chile.
EM avalenzuela.toro@gmail.com; pyensonn@si.edu; sgcarolina@gmail.com;
marioesuarezp@gmail.com
OI Gutstein, Carolina/0000-0002-0823-2434
FU CONICYT-PCHA/Magister Nacional [2013-221320410]; National Geographic
Society Committee on Research Exploration [9391-13]; National Museum of
Natural History (NMNH) Small Grant Award; NMNH Office of the Director;
Smithsonian Institution's Remington Kellogg Fund; National Geographic
Society Committee on Research Exploration grants [8903-11, 9019-11];
NMNH Imaging at the USNM; Smithsonian Institution Graduate Fellowship
FX This work is dedicated to the memory of the late Donald E. Hurlbert
(USNM), who photographed the type and paratype material of Australophoca
at the Smithsonian Institution, and will be remembered for his
dedication, kindness, artistry and humour across the institution. AVT
was funded by CONICYT-PCHA/Magister Nacional/2013-221320410, a Young
Explorer Grant (9391-13) from the National Geographic Society Committee
on Research Exploration and a Smithsonian Institution Graduate
Fellowship. Additional funding for this work comes from a National
Museum of Natural History (NMNH) Small Grant Award, discretionary
funding from NMNH Office of the Director, the Smithsonian Institution's
Remington Kellogg Fund, and two National Geographic Society Committee on
Research Exploration grants (8903-11, 9019-11) to NDP, and U-REDES
(Domeyko II UR-C12/1, Universidad de Chile) to the rest of the authors.
We would like to thank D. Rubilar-Rogers for the access to Fossil
Vertebrate collection of the Museo Nacional de Historia Natural (Chile),
and C. W. Potter, J. G. Mead, K. M. Helgen, J. J. Ososky and D. J.
Bohaska (all USNM) for access to Smithsonian collections of living and
fossil pinnipeds. We would also like to thank P. Kroehler, S. Jabo and
M. Pinsdorf (all USNM) for assistance with preparation of USNM material.
Additionally, we would like to thank M. Cozzuol and J. Velez-Juarbe for
providing comments and suggestions that improved a preliminary version
of the manuscript. Lastly, we are grateful for the support of the NMNH
Imaging at the USNM, including the late D. Hurlbert, J. Di Loreto, B.
Hance, K. N. Quarles, for photography of the type and paratype specimen
of Australophoca. We appreciate the useful and detailed comments from R.
W. Boessenecker, M. Churchill and S. Thomas, which substantially
improved this manuscript. This is contribution YEG (9391-13) # 2.
NR 98
TC 2
Z9 3
U1 0
U2 7
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 2056-2799
EI 2056-2802
J9 PAP PALAEONTOL
JI Pap. Palaeontol.
PD FEB
PY 2016
VL 2
IS 1
BP 101
EP 115
DI 10.1002/spp2.1033
PG 15
WC Paleontology
SC Paleontology
GA DD6TM
UT WOS:000370057400007
ER
PT J
AU Shizuka, D
Farine, DR
AF Shizuka, Daizaburo
Farine, Damien R.
TI Measuring the robustness of network community structure using
assortativity
SO ANIMAL BEHAVIOUR
LA English
DT Article
DE bootstrapping; community detection; flock; golden-crowned sparrow;
modularity; social network; thornbill; tit
ID ANIMAL SOCIAL NETWORKS; PHENOTYPIC ASSORTMENT; BEHAVIOR; ASSOCIATIONS;
ORGANIZATION; POPULATION; EVOLUTION; SELECTION; DYNAMICS; BIRDS
AB The existence of discrete social clusters, or 'communities', is a common feature of social networks in human and nonhuman animals. The level of such community structure in networks is typically measured using an index of modularity, Q. While modularity quantifies the degree to which individuals associate within versus between social communities and provides a useful measure of structure in the social network, it assumes that the network has been well sampled. However, animal social network data is typically subject to sampling errors. In particular, the associations among individuals are often not sampled equally, and animal social network studies are often based on a relatively small set of observations. Here, we extend an existing framework for bootstrapping network metrics to provide a method for assessing the robustness of community assignment in social networks using a metric we call community assortativity (r(com)). We use simulations to demonstrate that modularity can reliably detect the transition from random to structured associations in networks that differ in size and number of communities, while community assortativity accurately measures the level of confidence based on the detectability of associations. We then demonstrate the use of these metrics using three publicly available data sets of avian social networks. We suggest that by explicitly addressing the known limitations in sampling animal social network, this approach will facilitate more rigorous analyses of population-level structural patterns across social systems. (C) 2015 The Authors. Published on behalf of The Association for the Study of Animal Behaviour by Elsevier Ltd. This is an open access article under the CC BY license
C1 [Shizuka, Daizaburo] Univ Nebraska, Sch Biol Sci, 402 Manter Hall,1104 T St, Lincoln, NE 68588 USA.
[Farine, Damien R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford OX1 2JD, England.
[Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA USA.
[Farine, Damien R.] Smithsonian Trop Res Inst, Panama City, Panama.
[Farine, Damien R.] Max Planck Inst Ornithol, Dept Collect Behav, D-78457 Constance, Germany.
RP Shizuka, D (reprint author), Univ Nebraska, Sch Biol Sci, 402 Manter Hall,1104 T St, Lincoln, NE 68588 USA.
EM dshizuka2@unl.edu
FU National Science Foundation (NSF) [IOS1250895]; Biotechnology and
Biological Sciences Research Council (BBSRC) [BB/L006081/1]
FX We thank the organizers of the National Institute for Mathematical and
Biological Synthesis (NIMBioS) Investigative Workshop on Animal Social
Networks, which initiated this collaboration. D.S. thanks Bruce Lyon and
Alexis Chaine for their involvement in the empirical research that
inspired the development of these analytical methods. We thank the teams
of field assistants involved in collecting the empirical data we use
here. D.R.F. was funded by grants from the National Science Foundation
(NSF-IOS1250895) to Margaret Crofoot and the Biotechnology and
Biological Sciences Research Council (BBSRC: BB/L006081/1) to Ben
Sheldon.
NR 52
TC 0
Z9 0
U1 9
U2 20
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
EI 1095-8282
J9 ANIM BEHAV
JI Anim. Behav.
PD FEB
PY 2016
VL 112
BP 237
EP 246
DI 10.1016/j.anbehav.2015.12.007
PG 10
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA DD0NX
UT WOS:000369617800028
ER
PT J
AU Villanueva-Gutierrez, R
Roubik, D
AF Villanueva-Gutierrez, Rogel
Roubik, David W.
TI More than protein? Bee-flower interactions and effects of disturbance
regimes revealed by rare pollen in bee nests
SO ARTHROPOD-PLANT INTERACTIONS
LA English
DT Article
DE Bee-flower networks; Centris; Competition; Drought; Hurricanes;
Megachile; Melittopalynology; Nectar sources; Oil flowers; Palynology;
Pollen residues
ID GENERALIST SOLITARY BEES; AFRICANIZED HONEY-BEE; AMINO-ACIDS;
HYMENOPTERA APIDAE; RAIN-FORESTS; POLLINATION; PLANTS; MEGACHILIDAE;
CENTRIDINI; RESOURCE
AB Bees and their host flower populations were studied by identifying pollen to species or genus, from trap nests where bees were reared. Rare plant species in bee diets, and disturbance regimes, have not previously been researched and are emphasized here. Two focal bee groups with one species each (Megachilidae and Apidae) were studied in a 500,000-ha tropical reserve in the Yucatan Peninsula nine complete years. The number of rare or major pollen species in nests had no statistical correlation; thus, rare pollen analysis complements study of major brood provisions. We found most nests (87 % Megachile zaptlana, 93 % Centris analis) contained rare pollen; only 12 % of the 438 nests contained major pollen alone. Rare pollen sometimes indicated an energy source rather than a scarce protein resource. Trichome nectar of Cydista, along with Ipomoea and Caesalpinia, were nectar sources. Malpighiaceae, despite lacking nectar, often provided the complete Centris diet. Considering rare pollen, only Centris responded to drought, or competition from immigrant honeybees. Neither bee responded to hurricanes. Drought years coincided with low bee populations; Centris nests contained more rare species then. After feral Africanized honeybees colonized, Centris had more major species and fewer rare. Some herbarium vouchers from the study area contained exotic pollen, demonstrating in situ floral contamination and ecological generalization by bees, but this rarely occurred in plants found among the bee diets. Megachile and Centris responded differently to competition and resource scarcity, and plausibly evolved under different disturbance regimes, yet appeared well adapted to hurricane disturbance.
C1 [Villanueva-Gutierrez, Rogel] El Colegio Frontera Sur, Ave Centenario Km 5-5,Apdo Postal 424, Chetmal 77014, Quintana Roo, Mexico.
[Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Roubik, D (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
EM rvillanu@ecosur.mx; roubikd@si.edu
FU Smithsonian Institution
FX We thank Wilberto Colli Ucan and Margarito Tuz Novelo for their help in
fieldwork and with pollen acetolysis in the laboratory. Scholarly
Studies grants from the Smithsonian Institution provided financial
support; reviewers of API provided useful feedback.
NR 64
TC 0
Z9 0
U1 7
U2 21
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1872-8855
EI 1872-8847
J9 ARTHROPOD-PLANT INTE
JI Arthropod-Plant Interact.
PD FEB
PY 2016
VL 10
IS 1
BP 9
EP 20
DI 10.1007/s11829-015-9413-9
PG 12
WC Ecology; Entomology
SC Environmental Sciences & Ecology; Entomology
GA DC7UE
UT WOS:000369425100002
ER
PT J
AU Segura-Cox, DM
Harris, RJ
Tobin, JJ
Looney, LW
Li, ZY
Chandler, C
Kratter, K
Dunham, MM
Sadavoy, S
Perez, L
Melis, C
AF Segura-Cox, Dominique M.
Harris, Robert J.
Tobin, John J.
Looney, Leslie W.
Li, Zhi-Yun
Chandler, Claire
Kratter, Kaitlin
Dunham, Michael M.
Sadavoy, Sarah
Perez, Laura
Melis, Carl
TI THE VLA NASCENT DISK AND MULTIPLICITY SURVEY: FIRST LOOK AT RESOLVED
CANDIDATE DISKS AROUND CLASS 0 AND I PROTOSTARS IN THE PERSEUS MOLECULAR
CLOUD
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE protoplanetary disks; stars: protostars
ID MAGNETIC BRAKING CATASTROPHE; STAR-FORMING REGIONS; PROTOPLANETARY
DISKS; CIRCUMSTELLAR DISKS; OHMIC DISSIPATION; KEPLERIAN DISK; H2O
MASERS; CORES; ASTROMETRY; TURBULENCE
AB We present the first dust emission results toward a sample of seven protostellar disk candidates around Class 0 and I sources in the Perseus molecular cloud from the VLA Nascent Disk and Multiplicity (VANDAM) survey with similar to 0.'' 05 or 12 AU resolution. To examine the surface brightness profiles of these sources, we fit the Ka-band 8 mm dust-continuum data in the u, v-plane to a simple, parametrized model based on the Shakura-Sunyaev disk model. The candidate disks are well-fit by a model with a disk-shaped profile and have masses consistent with known Class 0 and I disks. The inner-disk surface densities of the VANDAM candidate disks have shallower density profiles compared to disks around more evolved Class II systems. The best-fit model radii of the seven early-result candidate disks are R-c > 10 AU; at 8 mm, the radii reflect lower limits on the disk size since dust continuum emission is tied to grain size and large grains radially drift inwards. These relatively large disks, if confirmed kinematically, are inconsistent with theoretical models where the disk size is limited by strong magnetic braking to <10 AU at early times.
C1 [Segura-Cox, Dominique M.; Harris, Robert J.; Looney, Leslie W.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Tobin, John J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Chandler, Claire; Perez, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Kratter, Kaitlin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Sadavoy, Sarah] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Segura-Cox, DM (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
EM segurac2@illinois.edu
FU NRAO Student Observing Support grant [SBC NRAO 2015-06997]; Netherlands
Organisation for Scientific Research (NWO) [639.041.439]; NASA
[NNX14AB38G]; NSF [AST-1313083]
FX D.M.S.C. is currently supported by NRAO Student Observing Support grant
SBC NRAO 2015-06997. J.J.T. is currently supported by grant 639.041.439
from the Netherlands Organisation for Scientific Research (NWO). Z.Y.L.
is supported by NASA NNX14AB38G and NSF AST-1313083.
NR 40
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2016
VL 817
IS 2
AR L14
DI 10.3847/2041-8205/817/2/L14
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7LB
UT WOS:000369400300004
ER
PT J
AU Tajfirouze, E
Reale, F
Peres, G
Testa, P
AF Tajfirouze, E.
Reale, F.
Peres, G.
Testa, P.
TI EUV FLICKERING OF SOLAR CORONAL LOOPS: A NEW DIAGNOSTIC OF CORONAL
HEATING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: UV radiation
ID FLARING ACTIVE-REGION; HOT PLASMA; EMISSION; HINODE/EIS
AB A previous work of ours found the best agreement between EUV light curves observed in an active region core (with evidence of super-hot plasma) and those predicted from a model with a random combination of many pulse-heated strands with a power-law energy distribution. We extend that work by including spatially resolved strand modeling and by studying the evolution of emission along the loops in the EUV 94 angstrom and 335 angstrom channels of the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Using the best parameters of the previous work as the input of the present one, we find that the amplitude of the random fluctuations driven by the random heat pulses increases from the bottom to the top of the loop in the 94 angstrom channel and from the top to the bottom in the 335 angstrom channel. This prediction is confirmed by the observation of a set of aligned neighboring pixels along a bright arc of an active region core. Maps of pixel fluctuations may therefore provide easy diagnostics of nanoflaring regions.
C1 [Tajfirouze, E.; Reale, F.; Peres, G.] Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Reale, F.; Peres, G.] INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Testa, P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Reale, F (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy.; Reale, F (reprint author), INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM reale@astropa.unipa.it
OI Reale, Fabio/0000-0002-1820-4824
FU italian Ministero dell'Universita e Ricerca; Lockheed-Martin
[SP02H1701R]; NASA [NNX15AF50G]
FX We thank the referee for constructive comments. E.T., F.R., and G.P.
acknowledge support from italian Ministero dell'Universita e Ricerca.
P.T. was supported by contract SP02H1701R from Lockheed-Martin to the
Smithsonian Astrophysical Observatory, and by NASA grant NNX15AF50G. SDO
data supplied courtesy of the SDO/AIA consortia. SDO is the first
mission to be launched for NASA's Living With a Star (LWS) Program.
NR 28
TC 3
Z9 3
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2016
VL 817
IS 2
AR L11
DI 10.3847/2041-8205/817/2/L11
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7LB
UT WOS:000369400300001
ER
PT J
AU Powell, LL
Wolfe, JD
Johnson, EI
Stouffer, PC
AF Powell, Luke L.
Wolfe, Jared D.
Johnson, Erik I.
Stouffer, Philip C.
TI Forest recovery in post-pasture Amazonia: Testing a conceptual model of
space use by insectivorous understory birds
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Antthrush; Fragmentation; Home range; Secondary forest; Telemetry;
Woodcreeper
ID ANIMAL MOVEMENT PATHS; RAIN-FOREST; BRAZILIAN AMAZONIA; FRACTAL
DIMENSION; HOME-RANGE; GENE FLOW; FRAGMENTS; SECONDARY; DEFORESTATION;
DISTRIBUTIONS
AB Understanding how animals move in a complex habitat mosaic is critical to biodiversity conservation as deforested lands and secondary rainforests accumulate in landscapes previously dominated by primary forests. To visualize the spatiotemporal dynamics of secondary forest recovery after pasture abandonment, we formed a conceptual model predicting avian space use during a temporal sequence beginning with deforestation and continuing through regrowth of old secondary forest. We tested five predictions of the model at the Biological Dynamics of Forest Fragments Project near Manaus, Brazil, using 73 radio-tagged understory insectivores of three species: two woodcreepers (Glyphorynchus spirurus, Xiphorhynchus pardalotus) and a terrestrial antthrush (Formicarius colma). Both woodcreepers provided evidence to support all predictions except that of greater path tortuosity in primary forest. Woodcreepers using secondary forest had larger home ranges, larger core areas, and faster movement rates than in primary forest Further, the proportion of all species' core areas in primary forest exceeded the proportion of home ranges in primary forest. Formicarius colma showed a fundamentally different pattern than the woodcreepers: it essentially avoided secondary forest until 27-31 years after pasture abandonment, at which point movements were indistinguishable from those in primary forest. Formicarius colma and other terrestrial insectivores show implastic spatiotemporal responses to recovering secondary growth, which we suspect contributes to the sensitivity of this guild to forest disturbance. Quantifying the value of marginal (and economically inconsequential) habitats such as secondary forest will be essential as land managers strive to maintain species persistence and connectivity in increasingly heterogeneous tropical landscapes. Published by Elsevier Ltd.
C1 Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, CP 478, BR-69011097 Manaus, AM, Brazil.
Louisiana State Univ, Sch Renewable Nat Resources, RNR 227, Baton Rouge, LA 70803 USA.
Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA.
[Wolfe, Jared D.] US Forest Serv, Redwood Sci Lab, Arcata, CA 95521 USA.
[Johnson, Erik I.] Natl Audubon Soc, 6160 Perkins Rd, Baton Rouge, LA 70808 USA.
RP Powell, LL (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zoolog Pk, Washington, DC 20013 USA.
EM Luke.L.Powell@gmail.com
FU National Science Foundation [LTREB 0545491]; American Union of
Ornithologists' Research Award; American Union of Ornithologists' Frank
M. Chapman Award; Wilson Ornithological Society's Paul A Stewart Award;
American Philosophical Society's Lewis Clark Fund
FX LLP would like to dedicate this paper to the memory of his Master's
adviser Bill Glanz, whose enthusiasm for the natural world was an
inspiration to all who knew him. We thank Marconi Cerqueira, Elizabeth
Condon, Paul Des Brisay, Camila Duarte, Gilberto Fernandez Arellano,
Jairo Lopes, Alercio Marajo de Reis, Rachelle McLaughlin, Karl Mokross,
Osmaildo, Aida Rodrigues, and Tatiana Straatmann for their contributions
in the field. The LSU "Bird Lunch" group, Kristina Cockle, Kyle Harms,
Jim Hines, Michael Kaller, Curtis Marantz, Michael Lefsky, Michael
Patten, Scott Saleska, Stefan Woltmann, and J. Van Remsen had important
contributions, including insightful reviews and advice on data analyses.
James Nichols helped us analyze differences in proportions of home
ranges and core areas in primary forest. We thank the following funding
sources: National Science Foundation's Long Term Ecological Research
grant in Biology (LTREB 0545491), American Union of Ornithologists'
Research Award, the American Union of Ornithologists' Frank M. Chapman
Award, the Wilson Ornithological Society's Paul A Stewart Award, and the
American Philosophical Society's Lewis & Clark Fund. We conducted this
research under LSU Institutional Animal Care and Use Committee approval
and under applicable Brazilian permits. This is publication number 681
in the BDFFP technical series and number 40 in the Amazonian ornithology
technical series. This manuscript was approved for publication by the
Director of the Louisiana Agricultural Experimental Station as
manuscript number 2015-241-22757.
NR 63
TC 0
Z9 0
U1 9
U2 40
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
EI 1873-2917
J9 BIOL CONSERV
JI Biol. Conserv.
PD FEB
PY 2016
VL 194
BP 22
EP 30
DI 10.1016/j.biocon.2015.11.025
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC8FW
UT WOS:000369456300003
ER
PT J
AU Stieb, DM
Chen, L
Beckerman, BS
Jerrett, M
Crouse, DL
Omariba, DWR
Peters, PA
van Donkelaar, A
Martin, RV
Burnett, RT
Gilbert, NL
Tjepkema, M
Liu, SL
Dugandzic, RM
AF Stieb, David M.
Chen, Li
Beckerman, Bernardo S.
Jerrett, Michael
Crouse, Daniel L.
Omariba, D. Walter Rasugu
Peters, Paul A.
van Donkelaar, Aaron
Martin, Randall V.
Burnett, Richard T.
Gilbert, Nicolas L.
Tjepkema, Michael
Liu, Shiliang
Dugandzic, Rose M.
TI Associations of Pregnancy Outcomes and PM2.5 in a National Canadian
Study
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
ID AMBIENT AIR-POLLUTION; NEIGHBORHOOD SOCIOECONOMIC-STATUS; LONG-TERM
EXPOSURE; LOW-BIRTH-WEIGHT; PRETERM BIRTH; MATERNAL EDUCATION; PREMATURE
BIRTH; LOS-ANGELES; HEALTH; DISPARITIES
AB BACKGROUND: Numerous studies have examined associations between air pollution and pregnancy outcomes, but most have been restricted to urban populations living near monitors.
OBJECTIVES: We examined the association between pregnancy outcomes and fine particulate matter in a large national study including urban and rural areas.
METHODS: Analyses were based on approximately 3 million singleton live births in Canada between 1999 and 2008. Exposures to PM2.5 (particles of median aerodynamic diameter <= 2.5 mu m) were assigned by mapping the mother's postal code to a monthly surface based on a national land use regression model that incorporated observations from fixed-site monitoring stations and satellite-derived estimates of PM2.5. Generalized estimating equations were used to examine the association between PM2.5 and preterm birth (gestational age < 37 weeks), term low birth weight (< 2,500 g), small for gestational age (SGA; < 10th percentile of birth weight for gestational age), and term birth weight, adjusting for individual covariates and neighborhood socioeconomic status (SES).
RESULTS: In fully adjusted models, a 10-mu g/m3 increase in PM2.5 over the entire pregnancy was associated with SGA (odds ratio = 1.04; 95% CI 1.01, 1.07) and reduced term birth weight (-20.5 g; 95% CI -24.7, -16.4). Associations varied across subgroups based on maternal place of birth and period (1999-2003 vs. 2004-2008).
CONCLUSIONS: This study, based on approximately 3 million births across Canada and employing PM2.5 estimates from a national spatiotemporal model, provides further evidence linking PM2.5 and pregnancy outcomes.
C1 [Stieb, David M.] Hlth Canada, Populat Studies Div, 445-757 West Hastings St Fed Tower, Vancouver, BC V6C 1A1, Canada.
[Chen, Li; Burnett, Richard T.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada.
[Beckerman, Bernardo S.] Univ Calif Berkeley, Sch Publ Hlth, Geog Informat Hlth & Exposure Sci Lab GIS HEAL, Berkeley, CA 94720 USA.
[Jerrett, Michael] Univ Calif Los Angeles, Fielding Sch Publ Hlth, Dept Environm Hlth Sci, Los Angeles, CA USA.
[Crouse, Daniel L.; Peters, Paul A.] Univ New Brunswick, Dept Sociol, Fredericton, NB, Canada.
[Omariba, D. Walter Rasugu] STAT Canada, Special Surveys Div, Ottawa, ON, Canada.
[van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Gilbert, Nicolas L.] Publ Hlth Agcy Canada, Vaccine & Immunizat Program Surveillance Div, Ottawa, ON, Canada.
[Tjepkema, Michael] STAT Canada, Hlth Anal Div, Ottawa, ON, Canada.
[Liu, Shiliang] Publ Hlth Agcy Canada, Surveillance & Epidemiol Div, Maternal Child & Youth Hlth, Ottawa, ON, Canada.
[Dugandzic, Rose M.] Hlth Canada, Air Hlth Sci Div, Ottawa, ON K1A 0L2, Canada.
RP Stieb, DM (reprint author), Hlth Canada, Populat Studies Div, 445-757 West Hastings St Fed Tower, Vancouver, BC V6C 1A1, Canada.
EM dave.stieb@hc-sc.gc.ca
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU Health Canada; Centers for Disease Control and Prevention
[200-2010-37394]; National Institute of Environmental Health Science
[5R01ES019573-04]
FX Funding was provided by Health Canada and, for some aspects of the work,
by Centers for Disease Control and Prevention award 200-2010-37394, and
by National Institute of Environmental Health Science grant
5R01ES019573-04.
NR 28
TC 6
Z9 7
U1 6
U2 17
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
EI 1552-9924
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD FEB
PY 2016
VL 124
IS 2
BP 243
EP 249
DI 10.1289/ehp.1408995
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA DC6NX
UT WOS:000369337900018
PM 26090691
ER
PT J
AU McKeon, CS
Weber, MX
Alter, SE
Seavy, NE
Crandall, ED
Barshis, DJ
Fechter-Leggett, ED
Oleson, KLL
AF McKeon, C. Seabird
Weber, Michele X.
Alter, S. Elizabeth
Seavy, Nathaniel E.
Crandall, Eric D.
Barshis, Daniel J.
Fechter-Leggett, Ethan D.
Oleson, Kirsten L. L.
TI Melting barriers to faunal exchange across ocean basins
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE arctic; biodiversity; birds; marine mammals; range shift
ID AMERICAN BIOTIC INTERCHANGE; ARCTIC MARINE MAMMALS; NORTH-ATLANTIC;
SEA-ICE; GRAY WHALES; ECOSYSTEM ENGINEERS; BALAENA-MYSTICETUS; BOWHEAD
WHALES; CLIMATE-CHANGE; PACIFIC-OCEAN
AB Accelerated loss of sea ice in the Arctic is opening routes connecting the Atlantic and Pacific Oceans for longer periods each year. These changes may increase the ease and frequency with which marine birds and mammals move between the Pacific and Atlantic Ocean basins. Indeed, recent observations of birds and mammals suggest these movements have intensified in recent decades. Reconnection of the Pacific and Atlantic Ocean basins will present both challenges to marine ecosystem conservation and an unprecedented opportunity to examine the ecological and evolutionary consequences of interoceanic faunal exchange in real time. To understand these changes and implement effective conservation of marine ecosystems, we need to further develop modeling efforts to predict the rate of dispersal and consequences of faunal exchange. These predictions can be tested by closely monitoring wildlife dispersal through the Arctic Ocean and using modern methods to explore the ecological and evolutionary consequences of these movements.
C1 [McKeon, C. Seabird] Natl Museum Nat Hist, Smithsonian Inst, Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Weber, Michele X.] Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA.
[Alter, S. Elizabeth] CUNY York Coll, Dept Biol, Jamaica, NY 11451 USA.
[Alter, S. Elizabeth] CUNY, Grad Ctr, Jamaica, NY 11451 USA.
[Seavy, Nathaniel E.] Point Blue Conservat Sci, 3820 Cypress Dr,Suite 11, Petaluma, CA 94954 USA.
[Crandall, Eric D.] UC Santa Cruz Inst Marine Sci, 110 Shaffer Rd, Santa Cruz, CA 95060 USA.
[Barshis, Daniel J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
[Fechter-Leggett, Ethan D.] Natl Inst Occupat Safety & Hlth, Resp Hlth Div, 1095 Willowdale Rd,MS 2800, Morgantown, WV 26505 USA.
[Oleson, Kirsten L. L.] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, 1910 East West Rd,Sherman 101, Honolulu, HI 96822 USA.
RP McKeon, CS (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
EM mckeons@si.edu
NR 69
TC 0
Z9 0
U1 8
U2 38
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD FEB
PY 2016
VL 22
IS 2
BP 465
EP 473
DI 10.1111/gcb.13116
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC3RC
UT WOS:000369135400001
PM 26618788
ER
PT J
AU Townsend, AK
Cooch, EG
Sillett, TS
Rodenhouse, NL
Holmes, RT
Webster, MS
AF Townsend, Andrea K.
Cooch, Evan G.
Sillett, T. Scott
Rodenhouse, Nicholas L.
Holmes, Richard T.
Webster, Michael S.
TI The interacting effects of food, spring temperature, and global climate
cycles on population dynamics of a migratory songbird
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE Black-throated blue warbler; climate change; El Nino Southern
Oscillation; mark-recapture; migratory songbird; phenotypic mismatch;
population dynamics; Pradel models; recruitment; Setophaga caerulescens
ID WARBLERS DENDROICA-CAERULESCENS; EL NINO/SOUTHERN OSCILLATION;
NORTH-ATLANTIC OSCILLATION; NINO-SOUTHERN-OSCILLATION; LONG-TERM;
MARK-RECAPTURE; NEOTROPICAL MIGRANT; AVIAN POPULATION; MODEL SELECTION;
BIRD POPULATION
AB Although long-distance migratory songbirds are widely believed to be at risk from warming temperature trends, species capable of attempting more than one brood in a breeding season could benefit from extended breeding seasons in warmer springs. To evaluate local and global factors affecting population dynamics of the black-throated blue warbler (Setophaga caerulescens), a double-brooded long-distance migrant, we used Pradel models to analyze 25years of mark-recapture data collected in New Hampshire, USA. We assessed the effects of spring temperature (local weather) and the El Nino Southern Oscillation index (a global climate cycle), as well as predator abundance, insect biomass, and local conspecific density on population growth in the subsequent year. Local and global climatic conditions affected warbler populations in different ways. We found that warbler population growth was lower following El Nino years (which have been linked to poor survival in the wintering grounds and low fledging weights in the breeding grounds) than La Nina years. At a local scale, populations increased following years with warm springs and abundant late-season food, but were unaffected by spring temperature following years when food was scarce. These results indicate that the warming temperature trends might have a positive effect on recruitment and population growth of black-throated blue warblers if food abundance is sustained in breeding areas. In contrast, potential intensification of future El Nino events could negatively impact vital rates and populations of this species.
C1 [Townsend, Andrea K.] Hamilton Coll, Dept Biol, Clinton, NY 13323 USA.
[Townsend, Andrea K.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA.
[Townsend, Andrea K.; Webster, Michael S.] Cornell Univ, Cornell Lab Ornithol, Ithaca, NY 14853 USA.
[Townsend, Andrea K.; Webster, Michael S.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA.
[Cooch, Evan G.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA.
[Rodenhouse, Nicholas L.] Wellesley Coll, Dept Biol Sci, Wellesley, MA 02482 USA.
[Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA.
RP Townsend, AK (reprint author), Hamilton Coll, Dept Biol, Clinton, NY 13323 USA.
EM aktownse@hamilton.edu
FU National Science Foundation (NSF); U.S. National Science Foundation
FX We thank the many students and field assistants who have worked with us
over the past 25 years. This research was supported by a Biological
Informatics Fellowship from the National Science Foundation (NSF) to AKT
and from NSF grants to Dartmouth College, Wellesley College, Cornell
University, and the Smithsonian Institution. We also acknowledge the
very helpful comments and suggestions from three anonymous reviewers and
the editor. This manuscript is a contribution of the Hubbard Brook
Ecosystem Study. Hubbard Brook is part of the Long-Term Ecological
Research (LTER) network, which is supported by the U.S. National Science
Foundation. The Hubbard Brook Experimental Forest is operated and
maintained by the USDA Forest Service, Northern Research Station,
Newtown Square, PA.
NR 86
TC 2
Z9 2
U1 28
U2 67
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD FEB
PY 2016
VL 22
IS 2
BP 544
EP 555
DI 10.1111/gcb.13053
PG 12
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC3RC
UT WOS:000369135400006
PM 26242236
ER
PT J
AU Wcislo, P
Gordon, IE
Cheng, CF
Hu, SM
Ciurylo, R
AF Wcislo, P.
Gordon, I. E.
Cheng, C. -F.
Hu, S. -M.
Ciurylo, R.
TI Collision-induced line-shape effects limiting the accuracy in
Doppler-limited spectroscopy of H-2
SO PHYSICAL REVIEW A
LA English
DT Article
ID ELECTRIC QUADRUPOLE TRANSITIONS; RING-DOWN SPECTROSCOPY; OPTICAL
FREQUENCY-MEASUREMENT; BROADENED ABSORPTION-LINE; CAVITY RING; SPEED
DEPENDENCE; MU-M; SPECTROMETER; PROFILES; BAND
AB Recent advances in theoretical calculations of H-2 dissociation energies and ultra-accurate measurements of H2 transition frequencies give possibilities not only for testing QED and relativistic effects, but also for searching for physics beyond the standard model. In this paper we show that at the level of 10(-4) cm(-1) the uncertainty of the Doppler-limited H-2 line position determination is dominated by collisional line-shape effects. We question the paradigm that the unperturbed transition energy can be determined from linear extrapolation of the line shift to zero pressure.
C1 [Wcislo, P.; Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
[Wcislo, P.; Ciurylo, R.] Nicolaus Copernicus Univ, Inst Phys, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland.
[Cheng, C. -F.; Hu, S. -M.] Univ Sci & Technol China, iChEM, Hefei Natl Lab Phys Sci Microscale, Hefei 230026, Peoples R China.
RP Wcislo, P (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM piotr.wcislo@fizyka.umk.pl
RI Hu, Shuiming/C-4287-2008; Ciurylo, Roman/G-8680-2014; Wcislo,
Piotr/C-9562-2015
OI Hu, Shuiming/0000-0002-1565-8468; Wcislo, Piotr/0000-0001-7909-4473
FU National Science Centre, Poland [DEC-2013/09/N/ST4/00327]; Foundation
for Polish Science START program; Fulbright Junior Research Award Grant;
Foundation for Polish Science TEAM Project; EU European Regional
Development Fund; Natural Science Foundation of China [21225314]; NASA
[NNX14AI55G]
FX P.W. was supported by the National Science Centre, Poland, Project No.
DEC-2013/09/N/ST4/00327, Foundation for Polish Science START program,
and the Fulbright Junior Research Award Grant. The research was part of
the program of the National Laboratory FAMO in Torun, Poland. The
research was partially supported by the Foundation for Polish Science
TEAM Project cofinanced by the EU European Regional Development Fund.
S.-M.H. was supported by the Natural Science Foundation of China (Grant
No. 21225314). I.E.G. was supported through NASA Grant No. NNX14AI55G.
NR 64
TC 1
Z9 1
U1 5
U2 15
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD FEB 1
PY 2016
VL 93
IS 2
AR 022501
DI 10.1103/PhysRevA.93.022501
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DC6XY
UT WOS:000369364100009
ER
PT J
AU Chisholm, RA
Wijedasa, LS
Swinfield, T
AF Chisholm, Ryan A.
Wijedasa, Lahiru S.
Swinfield, Tom
TI The need for long-term remedies for Indonesia's forest fires
SO CONSERVATION BIOLOGY
LA English
DT Letter
ID SOUTHEAST-ASIA; HAZE; PEAT
C1 [Chisholm, Ryan A.; Wijedasa, Lahiru S.] Natl Univ Singapore, Dept Biol Sci, Fac Sci, 14 Sci Dr 4, Singapore 117543, Singapore.
[Chisholm, Ryan A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Wijedasa, Lahiru S.] Conservat Links, 433,Clementi Ave 3,01-258, Singapore 120433, Singapore.
[Swinfield, Tom] Royal Soc Protect Birds, Ctr Conservat Sci, Sandy SG19 2DL, Beds, England.
[Swinfield, Tom] PT Restorasi Ekosistem Indonesia, Jl Kopral Hambali 120, Kel Pal Merah Lama 36139, Jambi, Indonesia.
RP Chisholm, RA (reprint author), Natl Univ Singapore, Dept Biol Sci, Fac Sci, 14 Sci Dr 4, Singapore 117543, Singapore.; Chisholm, RA (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
EM ryan.chis@gmail.com
NR 9
TC 10
Z9 10
U1 10
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD FEB
PY 2016
VL 30
IS 1
BP 5
EP 6
DI 10.1111/cobi.12662
PG 2
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC0WG
UT WOS:000368938000001
PM 26612785
ER
PT J
AU Schachat, SR
Mulcahy, DG
Mendelson, JR
AF Schachat, Sandra R.
Mulcahy, Daniel G.
Mendelson, Joseph R., III
TI Conservation threats and the phylogenetic utility of IUCN Red List
rankings in Incilius toads
SO CONSERVATION BIOLOGY
LA English
DT Article
DE amphibian; Bufonidae; extinction threat; Mesoamerica; phylogeny
ID EXTINCTION RISK; MAMMALIAN EXTINCTION; AMPHIBIAN DECLINES; ANURA
BUFONIDAE; SIGNAL; PATTERNS; TRAITS; FROGS; HISTORY; FUTURE
AB Phylogenetic analysis of extinction threat is an emerging tool in the field of conservation. However, there are problems with the methods and data as commonly used. Phylogenetic sampling usually extends to the level of family or genus, but International Union for Conservation of Nature (IUCN) rankings are available only for individual species, and, although different species within a taxonomic group may have the same IUCN rank, the species may have been ranked as such for different reasons. Therefore, IUCN rank may not reflect evolutionary history and thus may not be appropriate for use in a phylogenetic context. To be used appropriately, threat-risk data should reflect the cause of extinction threat rather than the IUCN threat ranking. In a case study of the toad genus Incilius, with phylogenetic sampling at the species level (so that the resolution of the phylogeny matches character data from the IUCN Red List), we analyzed causes of decline and IUCN threat rankings by calculating metrics of phylogenetic signal (such as Fritz and Purvis' D). We also analyzed the extent to which cause of decline and threat ranking overlap by calculating phylogenetic correlation between these 2 types of character data. Incilius species varied greatly in both threat ranking and cause of decline; this variability would be lost at a coarser taxonomic resolution. We found far more phylogenetic signal, likely correlated with evolutionary history, for causes of decline than for IUCN threat ranking. Individual causes of decline and IUCN threat rankings were largely uncorrelated on the phylogeny. Our results demonstrate the importance of character selection and taxonomic resolution when extinction threat is analyzed in a phylogenetic context.
C1 [Schachat, Sandra R.] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA.
[Schachat, Sandra R.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, POB 37012,MRC 121, Washington, DC 20013 USA.
[Mulcahy, Daniel G.] Smithsonian Inst, Global Genome Initiat, Natl Museum Nat Hist, POB 37012,MRC 183, Washington, DC 20013 USA.
[Mendelson, Joseph R., III] Zoo Atlanta, 800 Cherokee Ave SE, Atlanta, GA 30315 USA.
[Mendelson, Joseph R., III] Georgia Inst Technol, Sch Biol, 301 Ferst Dr, Atlanta, GA 30332 USA.
RP Mendelson, JR (reprint author), Zoo Atlanta, 800 Cherokee Ave SE, Atlanta, GA 30315 USA.; Mendelson, JR (reprint author), Georgia Inst Technol, Sch Biol, 301 Ferst Dr, Atlanta, GA 30332 USA.
EM jmendelson@zooatlanta.org
OI Schachat, Sandra/0000-0003-3237-5619
FU National Science Foundation Graduate Research Fellowship Program
[DGE-1125191]
FX We thank J.C. Maerz, A. Belasen, C. VanBuren, and two anonymous
reviewers for constructive feedback and discussions. S.R.S. is supported
by the National Science Foundation Graduate Research Fellowship Program
under grant DGE-1125191.
NR 45
TC 1
Z9 1
U1 2
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD FEB
PY 2016
VL 30
IS 1
BP 72
EP 81
DI 10.1111/cobi.12567
PG 10
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC0WG
UT WOS:000368938000009
PM 26243724
ER
PT J
AU Chollett, I
Box, SJ
Mumby, PJ
AF Chollett, Iliana
Box, Stephen J.
Mumby, Peter J.
TI Quantifying the squeezing or stretching of fisheries as they adapt to
displacement by marine reserves
SO CONSERVATION BIOLOGY
LA English
DT Article
DE displacement; Honduras; inherent mobility; imposed mobility; marine
protected area; set theory
ID FISHING EFFORT; PROTECTED AREAS; HIGH-RESOLUTION; FLEET DYNAMICS; ZONING
CHANGES; MANAGEMENT; CONSEQUENCES; CLOSURES; BEHAVIOR; CATCH
AB The designation of no-take marine reserves involves social and economic concerns due to the resulting displacement of fishing effort, when fishing rights are removed from those who traditionally fished within an area. Displacement can influence the functioning of the fishery and success of the reserve, yet levels of displacement are seldom quantified after reserve implementation and very rarely before that. We devised a simple analytical framework based on set theory to facilitate reserve placement. Implementation of the framework requires maps of fishing grounds, fishing effort, or catch per unit effort for at least 2 years. The framework quantifies the level of conflict that a reserve designation might cause in the fishing sector due to displacement and the opportunities to offset the conflict through fisher spatial mobility (i.e., ability of fishers to fish elsewhere). We also considered how the outputs of the framework can be used to identify targeted management interventions for each fishery. We applied the method in Honduras, where the largest marine protected area in Central America is being placed, for which spatial data on fishing effort were available for 6 fisheries over 3 years. The proposed closure had a greater negative impact on the shrimp and lobster scuba fisheries, which concentrated respectively 28% and 18% of their effort inside the reserve. These fisheries could not accommodate the displacement within existing fishing grounds. Both would be forced to stretch into new fishing grounds, which are available but are of unknown quality. These stakeholders will likely require compensation to offset costly exploratory fishing or to travel to fishing grounds farther away from port.
C1 [Chollett, Iliana; Box, Stephen J.] Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
[Chollett, Iliana; Mumby, Peter J.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4QD, Devon, England.
[Chollett, Iliana; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia.
RP Chollett, I (reprint author), Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.; Chollett, I (reprint author), Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4QD, Devon, England.; Chollett, I (reprint author), Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia.
EM iliana.chollett@gmail.com
FU European Union [244161]; Summit Foundation; Pew [2008-000330-010]; ARC
[FL0992179]
FX We received funding from the European Union 7th Framework Programme
(P7/2007-2013) under grant agreement 244161. I.C. and S.J.B. were
supported by The Summit Foundation. P.J.M was supported by Pew (grant
2008-000330-010) and ARC Laureate Fellowships (FL0992179). We thank
DIGEPESCA, particularly L. Alfaro, for granting access to the Honduran
VMS data. We are very grateful to M. Nunez from the Centro de Estudios
Marinos for carrying out data collection and to J. Varagne (Collecte
Localisation Satellites Group) for technical assistance in the
pre-processing of VMS data. This is Smithsonian Marine Station
Contribution number 1001.
NR 49
TC 1
Z9 1
U1 5
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD FEB
PY 2016
VL 30
IS 1
BP 166
EP 175
DI 10.1111/cobi.12573
PG 10
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DC0WG
UT WOS:000368938000018
PM 26096358
ER
PT J
AU Smith, FA
Tome, CP
Smith, EAE
Lyons, SK
Newsome, SD
Stafford, TW
AF Smith, Felisa A.
Tome, Catalina P.
Smith, Emma A. Elliott
Lyons, S. Kathleen
Newsome, Seth D.
Stafford, Thomas W.
TI Unraveling the consequences of the terminal Pleistocene megafauna
extinction on mammal community assembly
SO ECOGRAPHY
LA English
DT Article
ID LATE QUATERNARY EXTINCTIONS; NORTH-AMERICA; BODY-SIZE; STABLE-ISOTOPES;
CLIMATE-CHANGE; SOUTH-AMERICA; DIVERSITY; DIET; PATTERNS; HABITAT
AB Recent studies connecting the decline of large predators and consumers with the disintegration of ecosystems often overlook that this natural experiment already occurred. As recently as 14 ka, tens of millions of large-bodied mammals were widespread across the American continents. Within 1000 yr of the arrival of humans, approximate to 80% were extinct including all > 600 kg. While the cause of the late Pleistocene (LP) extinction remains contentious, largely overlooked are the ecological consequences of the loss of millions of large-bodied animals. Here, we examine the influence of the LP extinction on a local mammal community. Our study site is Hall's Cave in the Great Plains of Texas, which has unparalleled fine-grained temporal resolution over the past 20 ka, allowing characterization of the community before and after the extinction. In step with continental patterns, this community lost 80% of large-bodied herbivores and 20% of apex predators at the LP extinction. Using tightly constrained temporal windows spanning full glacial to modern time periods and comprehensive faunal lists, we reconstruct mammal associations and body size distributions over time. We find changes in alpha and beta diversity, and in the statistical moments associated with periods of climate change as well as with the LP extinction event. Additionally, there is a fundamental change in the composition of herbivores, with grazers being replaced by frugivores/granivores starting about 15 ka; the only large-bodied grazer remaining today is the bison Bison bison. Moreover, the null model program PAIRS reveals interesting temporal patterns in the disassociation or co-occurrence of species through the terminal Pleistocene and Holocene. Extinct species formed more significant associations than modern ones, and formed more aggregated pairs than do modern species. Further, negative species associations were about three times stronger than positive ones, suggesting that competitive interactions or environmental filtering are a strong force in community structure.
C1 [Smith, Felisa A.; Tome, Catalina P.; Smith, Emma A. Elliott; Newsome, Seth D.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Lyons, S. Kathleen] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Stafford, Thomas W.] Univ Aarhus, Dept Phys & Astron, Aarhus, Denmark.
RP Smith, FA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
EM fasmith@unm.edu
FU Evolution of Terrestrial Ecosystems Program at the National Museum of
Natural History; NSF-DEB [1257625]
FX We thank Chris Sagebiel, the Collections Manager at the Texas Memorial
Museum, and Professor/Curator Emeritus Extraordinaire Ernie Lundelius,
for their enthusiasm and assistance with this project, the Hall family
for generously allowing multiple excavations on their property, Meghan
Balk and Melissa Pardi for help with ice core and paleoclimate data,
Andrew Du with PAIRS analyses, and Aniko Toth for help with beta
diversity analysis. We are also grateful to the careful and
comprehensive work conducted by Richard Toomey, which jumpstarted our
efforts. Thanks also to the members of the Smith lab at UNM for their
enthusiasm and comments. Funding for SKL was provided by the Evolution
of Terrestrial Ecosystems Program at the National Museum of Natural
History and NSF-DEB 1257625.
NR 116
TC 0
Z9 0
U1 32
U2 56
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0906-7590
EI 1600-0587
J9 ECOGRAPHY
JI Ecography
PD FEB
PY 2016
VL 39
IS 2
BP 223
EP 239
DI 10.1111/ecog.01779
PG 17
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DB8UZ
UT WOS:000368793700013
ER
PT J
AU Liu, XQ
Ickert-Bond, SM
Nie, ZL
Zhou, Z
Chen, LQ
Wen, J
AF Liu, Xiu-Qun
Ickert-Bond, Stefanie M.
Nie, Ze-Long
Zhou, Zhuo
Chen, Long-Qing
Wen, Jun
TI Phylogeny of the Ampelocissus-Vitis Glade in Vitaceae supports the New
World origin of the grape genus
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Ampelocissus; Vitis; Grapes; Vitaceae; Biogeography
ID EASTERN NORTH-AMERICA; NUCLEAR RIBOSOMAL DNA; DISPERSAL-VICARIANCE
ANALYSIS; LONG-DISTANCE DISPERSAL; FAMILY VITACEAE; MOLECULAR PHYLOGENY;
HISTORICAL BIOGEOGRAPHY; INTERCONTINENTAL DISJUNCTIONS; SHOOT
ARCHITECTURE; CHLOROPLAST DNA
AB The grapes and the close allies in Vitaceae are of great agronomic and economic importance. Our previous studies showed that the grape genus Vitis was closely related to three tropical genera, which formed the Ampelocissus-Vitis Glade (including Vitis, Ampelocissus, Nothocissus and Pterisanthes). Yet the phylogenetic relationships of the four genera within this Glade remain poorly resolved. Furthermore, the geographic origin of Vitis is still controversial, because the sampling of the close relatives of Vitis was too limited in the previous studies. This study reconstructs the phylogenetic relationships within the Glade, and hypothesizes the origin of Vitis in a broader phylogenetic framework, using five plastid and two nuclear markers. The Ampelocissus-Vitis Glade is supported to be composed of five main lineages. Vitis includes two described subgenera each as a monophyletic group. Ampelocissus is paraphyletic. The New World Ampelocissus does not form a Glade and shows a complex phylogenetic relationship, with A. acapulcensis and A. javalensis forming a Glade, and A. erdvendbergiana sister to Vitis. The majority of the Asian Ampelocissus species form a Glade, within which Pterisanthes is nested. Pterisanthes is polyphyletic, suggesting that the lamellate inflorescence characteristic of the genus represents convergence. Nothocissus is sister to the Glade of Asian Ampelocissus and Pterisanthes. The African Ampelocissus forms a Glade with several Asian species. Based on the Bayesian dating and both the RASP and Lagrange analyses, Vitis is inferred to have originated in the New World during the late Eocene (39.4 Ma, 95% HPD: 32.6-48.6 Ma), then migrated to Eurasia in the late Eocene (37.3 Ma, 95% HPD: 30.9-45.1 Ma). The North Atlantic land bridges (NALB) are hypothesized to be the most plausible route for the Vitis migration from the New World to Eurasia, while intercontinental long distance dispersal (LDD) cannot be eliminated as a likely mechanism. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Liu, Xiu-Qun; Chen, Long-Qing] Huazhong Agr Univ, Coll Hort & Forestry Sci, Key Lab Hort Plant Biol, Minist Educ, Wuhan 430070, Peoples R China.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum North Herbarium, Fairbanks, AK 99775 USA.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA.
[Nie, Ze-Long] Jishou Univ, Coll Biol & Environm Sci, Key Lab Plant Resources Conservat & Utilizat, Jishou 416000, Peoples R China.
[Zhou, Zhuo] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Peoples R China.
[Wen, Jun] Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, MRC166, Washington, DC 20013 USA.
RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, MRC166, Washington, DC 20013 USA.
EM wenj@si.edu
RI Ickert-Bond, Stefanie/B-3216-2012;
OI Ickert-Bond, Stefanie/0000-0001-8198-8898; Liu,
Xiu-Qun/0000-0001-9655-6406
FU US National Science Foundation [DEB 0743474]; National Natural Science
Foundation of China [31370249]; Smithsonian Endowment Grant Program;
Small Grant Program of the National Museum of Natural History of the
Smithsonian Institution; John D. and Catherine T. MacArthur Foundation;
Natural Science Foundation of Hubei Province of China [2013CFB199];
Fundamental Research Funds for the Central Universities, China
[2011QC079]
FX We thank X.Z. Kan, Y. Meng, Deden Girmansyah and Y.M. Shui for
collecting leaf material or laboratory assistance and also acknowledge
support by the US National Science Foundation (DEB 0743474 to S.R.
Manchester and J. Wen), the National Natural Science Foundation of China
(Grant No. 31370249), the Smithsonian Endowment Grant Program, the Small
Grant Program of the National Museum of Natural History of the
Smithsonian Institution, and John D. and Catherine T. MacArthur
Foundation, the Natural Science Foundation of Hubei Province of China
(Grant No. 2013CFB199), and the Fundamental Research Funds for the
Central Universities, China (Program No. 2011QC079).
NR 140
TC 5
Z9 5
U1 5
U2 18
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
EI 1095-9513
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD FEB
PY 2016
VL 95
BP 217
EP 228
DI 10.1016/j.ympev.2015.10.013
PG 12
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA DC1JU
UT WOS:000368973400018
PM 26545592
ER
PT J
AU Wcislo, WT
AF Wcislo, William T.
TI Trophallaxis in weakly social bees (Apoidea)
SO ECOLOGICAL ENTOMOLOGY
LA English
DT Editorial Material
ID ORIGIN
C1 [Wcislo, William T.] Smithsonian Trop Res Inst, Apartado, Panama.
[Wcislo, William T.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.
RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.
EM WcisloW@si.edu
NR 23
TC 0
Z9 0
U1 2
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0307-6946
EI 1365-2311
J9 ECOL ENTOMOL
JI Ecol. Entomol.
PD FEB
PY 2016
VL 41
IS 1
BP 37
EP 39
DI 10.1111/een.12289
PG 3
WC Entomology
SC Entomology
GA DB4UE
UT WOS:000368508200006
ER
PT J
AU Aihara, I
de Silva, P
Bernal, XE
AF Aihara, Ikkyu
de Silva, Priyanka
Bernal, Ximena E.
TI Acoustic Preference of Frog-Biting Midges (Corethrella spp) Attacking
Tungara Frogs in their Natural Habitat
SO ETHOLOGY
LA English
DT Article
DE acoustic preferences; eavesdroppers; call rate; call complexity;
Physalemus
ID FEMALE MATE CHOICE; HYPEROLIUS-MARMORATUS; COURTSHIP SONG; FIELD
CRICKET; CALLING SONG; REED FROG; BEHAVIOR; LIGHT; ATTRACTION; CHORUSES
AB In many animals, males aggregate to produce mating signals that attract conspecific females. These leks, however, also attract eavesdropping predators and parasites lured by the mating signal. This study investigates the acoustic preferences of eavesdroppers attracted to natural choruses in a Neotropical frog, the tungara frog (Engystomops pustulosus). In particular, we examined the responses of frog-biting midges to natural variation in call properties and signaling rates of males in the chorus. These midges use the mating calls of the frogs to localize them and obtain a blood meal. Although it is known that the midges prefer complex over simple tungara frog calls, it is unclear how these eavesdroppers respond to natural call variation when confronted with multiple males in a chorus. We investigated the acoustic preference of the midges using calling frogs in their natural environment and thus accounted for natural variation in their call properties. We performed field recordings using a sound imaging system to quantify the temporal call properties of males in small choruses. During these recordings, we also collected frog-biting midges attacking calling males. Our results revealed that, in a given chorus, male frogs calling at higher rates and with higher call complexity attracted a larger number of frog-biting midges. Call rate was particularly important at increasing the number of midges attracted when males produced calls of lower complexity. Similarly, call complexity increased attractiveness to the midges especially when males produced calls at a low repetition rate. Given that female tungara frogs prefer calls produced at higher repetition rates and higher complexity, this study highlights the challenge faced by signalers when increasing attractiveness of the signal to their intended receivers.
C1 [Aihara, Ikkyu] Doshisha Univ, Fac Life & Med Sci, Dept Biomed Informat, Kyoto 6100394, Japan.
[de Silva, Priyanka] Univ Peradeniya, Fac Sci, Dept Zool, Peradeniya, Sri Lanka.
[Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA.
[Bernal, Ximena E.] Smithsonian Trop Res Inst, Gamboa, Panama.
RP Aihara, I (reprint author), Doshisha Univ, Fac Life & Med Sci, Dept Biomed Informat, Kyoto 6100394, Japan.
EM ikkyu.aihara@gmail.com
FU National Science Foundation [IOS-1258039/1433990]
FX We are grateful to M. Yasugi, M. Hoso, and T. Shimada for their valuable
advice on our analysis with GLMMs. We are also grateful to H. G. Okuno
for the support of the usage of a sound imaging system. The Smithsonian
Tropical Research Institute provided logistic support that made this
work possible. The Panamanian Environmental Agency, Autoridad National
del Medio Ambiente (ANAM), provided collection permits to perform this
work (SE/A-64-13). This work was supported by a National Science
Foundation grant (IOS-1258039/1433990) to X.E.B.
NR 33
TC 1
Z9 1
U1 7
U2 28
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0179-1613
EI 1439-0310
J9 ETHOLOGY
JI Ethology
PD FEB
PY 2016
VL 122
IS 2
BP 105
EP 113
DI 10.1111/eth.12452
PG 9
WC Psychology, Biological; Behavioral Sciences; Zoology
SC Psychology; Behavioral Sciences; Zoology
GA DB8ZF
UT WOS:000368805000002
ER
PT J
AU Yadav, RK
Gastine, T
Christensen, UR
Duarte, LDV
Reiners, A
AF Yadav, R. K.
Gastine, T.
Christensen, U. R.
Duarte, L. D. V.
Reiners, A.
TI Effect of shear and magnetic field on the heat-transfer efficiency of
convection in rotating spherical shells
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Numerical solutions; Dynamo: theories and simulations; Planetary
interiors
ID RAYLEIGH-BENARD CONVECTION; SPIRALING-COLUMNAR CONVECTION; ZONAL FLOW
DRIVEN; DIFFERENTIAL ROTATION; TURBULENT CONVECTION; THERMAL-CONVECTION;
PLANETARY CORES; MAJOR PLANETS; DYNAMO ACTION; SCALING LAWS
AB We study rotating thermal convection in spherical shells as prototype for flow in the cores of terrestrial planets, gas planets or in stars. We base our analysis on a set of about 450 direct numerical simulations of the (magneto) hydrodynamic equations under the Boussinesq approximation. The Ekman number ranges from 10(-3) to 10(-5). The supercriticality of the convection reaches about 1000 in some models. Four sets of simulations are considered: non-magnetic simulations and dynamo simulations with either free-slip or no-slip flow boundary conditions. The non-magnetic setup with free-slip boundaries generates the strongest zonal flows. Both non-magnetic simulations with no-slip flow boundary conditions and self-consistent dynamos with free-slip boundaries have drastically reduced zonal-flows. Suppression of shear leads to a substantial gain in heat-transfer efficiency, increasing by a factor of 3 in some cases. Such efficiency enhancement occurs as long as the convection is significantly influenced by rotation. At higher convective driving the heat-transfer efficiency tends towards that of the classical non-rotating Rayleigh-Benard system. Analysis of the latitudinal distribution of heat flow at the outer boundary reveals that the shear is most effective at suppressing heat-transfer in the equatorial regions. Simulations with convection zones of different thickness show that the zonal flows become less energetic in thicker shells, and, therefore, their effect on heat-transfer efficiency decreases. Furthermore, we explore the influence of the magnetic field on the non-zonal flow components of the convection. For this we compare the heat-transfer efficiency of no-slip non-magnetic cases with that of the no-slip dynamo simulations. We find that at E = 10(-5) magnetic field significantly affects the convection and a maximum gain of about 30 per cent (as compared to the non-magnetic case) in heat-transfer efficiency is obtained for an Elsasser number of about 3. Our analysis motivates us to speculate that convection in the polar regions in dynamos at E = 10(-5) is probably in a 'magnetostrophic' regime.
C1 [Yadav, R. K.; Gastine, T.; Christensen, U. R.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Yadav, R. K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Duarte, L. D. V.] Univ Exeter, Dept Phys & Astron, Exeter EX4 4SB, Devon, England.
[Reiners, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
RP Yadav, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rakesh.yadav@cfa.harvard.edu
RI Yadav, Rakesh/E-2169-2017
OI Yadav, Rakesh/0000-0002-9569-2438
FU Deutsche Forschungsgemeinschaft (DFG) [SFB 963/A17, 1488]; NASA
[GO4-15011X]; HLRN [nip00031]
FX We thank the reviewers, Julien Aubert and Robert Teed, for many useful
comments which greatly improved the presentation of the manuscript. We
also thank Jonathan Aurnou for interesting comments. We acknowledge
support from the Deutsche Forschungsgemeinschaft (DFG) through Project
SFB 963/A17 and the Special Priority Program 1488. RKY also acknowledges
support from NASA Chandra grant GO4-15011X. Computations were performed
on the GWDG computer facilities in Gottingen, Regionales Rechenzentrum
fur Niedersachsen, HLRN under project 'nip00031', and at Rechenzentrum
Garching (RZG). We also thank Tilman Dannert (RZG) for implementing MPI
and then hybrid OpenMP+MPI parallelization in MagIC.
NR 111
TC 7
Z9 7
U1 1
U2 6
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD FEB
PY 2016
VL 204
IS 2
BP 1120
EP 1133
DI 10.1093/gji/ggv506
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DB3QT
UT WOS:000368427100032
ER
PT J
AU Kapheim, KM
Chan, TY
Smith, AR
Wcislo, WT
Nonacs, P
AF Kapheim, K. M.
Chan, T. -Y.
Smith, A. R.
Wcislo, W. T.
Nonacs, P.
TI Ontogeny of division of labor in a facultatively eusocial sweat bee
Megalopta genalis
SO INSECTES SOCIAUX
LA English
DT Article
DE Dominance behavior; Megalopta genalis; Behavioral ontogeny; Division of
labor; Eusociality
ID LASIOGLOSSUM-ZEPHYRUM HYMENOPTERA; HALICTINE BEE; ECUADORIA HYMENOPTERA;
BEHAVIOR; COLONIES; SOLITARY; TROPHALLAXIS; WORKERS; QUEENS
AB In eusocial nests, colony task are divided among queens and workers, but how this division of labor develops is unknown for most species. We compared division of labor and aggressive behavior among queens and workers in the facultatively eusocial bee, Megalopta genalis, using nests with established queen-worker pairs and nests in which the incipient worker had recently emerged. We find that the majority of aggression is directed from queens toward workers in both incipient and established relationships. Established workers forage and perform trophallaxis as donors more frequently than queens, but both queens and workers perform trophallaxis as donors when workers are young. Queens spend significantly more time nest guarding than incipient and established workers, perhaps because older workers spend more time foraging and incipient workers spend significantly more time in cells than do queens. Our results show that the development of worker behavior involves dynamic temporal changes in task performance among queens and workers during the 10 days after worker emergence. During this establishment period, queens engage in maternal care by feeding their daughters, but are also aggressive toward them. This may be a mechanism by which queens coerce their daughters into becoming non-reproductive workers.
C1 [Kapheim, K. M.] Utah State Univ, Dept Biol, 5305 Old Main Hill, Logan, UT 84322 USA.
[Chan, T. -Y.; Nonacs, P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr South, Los Angeles, CA 90095 USA.
[Smith, A. R.] George Washington Univ, Dept Biol Sci, 800 22nd St NW,Suite 6000, Washington, DC 20052 USA.
[Wcislo, W. T.] Smithsonian Trop Res Inst, Apartado 0843, Balboa, Panama.
RP Kapheim, KM (reprint author), Utah State Univ, Dept Biol, 5305 Old Main Hill, Logan, UT 84322 USA.
EM karen.kapheim@usu.edu
FU NSF [DDIG-0808256, IOS-0642085]; Smithsonian Tropical Research Institute
(STRI); Smithsonian Institution; UCLA; AWIS; U.S. Dept. Ed.; STRI;
SENACYT [COL-06-030]
FX We thank M. Lopez-Uribe, M. Reiser, R. Cossio, D. La Rosa, J. Medina
Gutierrez, S. Bernal, D. Ramirez Garcia, T. Alvey for field assistance;
T. Innocent for help in designing the ethogram; A. Lee, C. Sheridan, H.
Denenberg, S. Dao, F. Choe, A. Bird, A. Espinosa, E. Anderson, R. Parks
for help in scoring the videos; O. Acevedo, B. Jimenez, O. Arosemena,
for logistical support. Research on BCI was conducted under A.N.A.M.
permit # SEX/A-34-09. K.M.K was supported by funds from NSF
DDIG-0808256, Smithsonian Tropical Research Institute (STRI),
Smithsonian Institution, UCLA, AWIS, U.S. Dept. Ed. K.M.K and P.N. were
supported by NSF grant IOS-0642085. W.T.W. and A.R.S. were supported by
STRI and SENACYT grant COL-06-030.
NR 32
TC 1
Z9 1
U1 3
U2 9
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0020-1812
EI 1420-9098
J9 INSECT SOC
JI Insect. Soc.
PD FEB
PY 2016
VL 63
IS 1
BP 185
EP 191
DI 10.1007/s00040-015-0454-y
PG 7
WC Entomology
SC Entomology
GA DB6RA
UT WOS:000368641500021
ER
PT J
AU Verheyen, K
Vanhellemont, M
Auge, H
Baeten, L
Baraloto, C
Barsoum, N
Bilodeau-Gauthier, S
Bruelheide, H
Castagneyrol, B
Godbold, D
Haase, J
Hector, A
Jactel, H
Koricheva, J
Loreau, M
Mereu, S
Messier, C
Muys, B
Nolet, P
Paquette, A
Parker, J
Perring, M
Ponette, Q
Potvin, C
Reich, P
Smith, A
Weih, M
Scherer-Lorenzen, M
AF Verheyen, Kris
Vanhellemont, Margot
Auge, Harald
Baeten, Lander
Baraloto, Christopher
Barsoum, Nadia
Bilodeau-Gauthier, Simon
Bruelheide, Helge
Castagneyrol, Bastien
Godbold, Douglas
Haase, Josephine
Hector, Andy
Jactel, Herve
Koricheva, Julia
Loreau, Michel
Mereu, Simone
Messier, Christian
Muys, Bart
Nolet, Philippe
Paquette, Alain
Parker, John
Perring, Mike
Ponette, Quentin
Potvin, Catherine
Reich, Peter
Smith, Andy
Weih, Martin
Scherer-Lorenzen, Michael
TI Contributions of a global network of tree diversity experiments to
sustainable forest plantations
SO AMBIO
LA English
DT Article
DE Biodiversity experiments; Functional biodiversity research; Plantation
forest; Sustainable forest management; Ecological restoration
ID CLIMATE-CHANGE; ECOSYSTEM SERVICES; BIODIVERSITY LOSS; TROPICAL FORESTS;
HERBIVORY; PRODUCTIVITY; INSECTS; DENSITY; BIOMASS; STANDS
AB The area of forest plantations is increasing worldwide helping to meet timber demand and protect natural forests. However, with global change, monospecific plantations are increasingly vulnerable to abiotic and biotic disturbances. As an adaption measure we need to move to plantations that are more diverse in genotypes, species, and structure, with a design underpinned by science. TreeDivNet, a global network of tree diversity experiments, responds to this need by assessing the advantages and disadvantages of mixed species plantations. The network currently consists of 18 experiments, distributed over 36 sites and five ecoregions. With plantations 1-15 years old, TreeDivNet can already provide relevant data for forest policy and management. In this paper, we highlight some early results on the carbon sequestration and pest resistance potential of more diverse plantations. Finally, suggestions are made for new, innovative experiments in understudied regions to complement the existing network.
C1 [Verheyen, Kris; Vanhellemont, Margot; Baeten, Lander; Perring, Mike] Univ Ghent, Dept Forest & Water Management, Forest & Nat Lab, B-9090 Melle Gontrode, Belgium.
[Auge, Harald] Helmholtz Ctr Environm Res, Dept Community Ecol, D-06120 Halle, Germany.
[Auge, Harald] German Ctr Integrat Biodivers Res Halle Jena Leip, iDiv, D-04103 Leipzig, Germany.
[Baraloto, Christopher] Florida Int Univ, Dept Biol Sci, Int Ctr Trop Bot, Miami, FL 33199 USA.
[Baraloto, Christopher] INRA, UMR Ecol Forets Guyane, Kourou 97310, French Guiana.
[Baraloto, Christopher] Inst Nacl de Pesquisas da Amazonia, Dept Bot, Manaus, Amazonas, Brazil.
[Barsoum, Nadia] Forest Res, Ctr Ecosyst Soc & Biosecur, Farnham GU10 4LH, Surrey, England.
[Bilodeau-Gauthier, Simon; Messier, Christian; Paquette, Alain] Univ Quebec, Ctr Forest Res, Ctr Ville Stn, Montreal, PQ, Canada.
[Bruelheide, Helge] Univ Halle Wittenberg, Inst Biol, Geobot & Bot Garden, D-06108 Halle, Germany.
[Castagneyrol, Bastien] INRA, UMR BIOGECO 1202, F-33612 Cestas, France.
[Castagneyrol, Bastien; Jactel, Herve] INRA, UMR BIOGECO 1202, F-33610 Cestas, France.
[Castagneyrol, Bastien; Jactel, Herve] Univ Bordeaux, BIOGECO, UMR 1202, F-33615 Pessac, France.
[Godbold, Douglas] Univ Bodenkultur BOKU, Inst Forest Ecol, A-1190 Vienna, Austria.
[Haase, Josephine] Univ Zurich, Inst Evolutionary Biol & Environm Studies, A-8057 Zurich, Austria.
[Haase, Josephine; Scherer-Lorenzen, Michael] Univ Freiburg, Fac Biol, D-79104 Freiburg, Germany.
[Haase, Josephine] ETH, Dept Environm Syst Sci, Ecosyst Management, CH-8092 Zurich, Switzerland.
[Hector, Andy] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England.
[Koricheva, Julia] Royal Holloway Univ London, Sch Biol Sci, Egham TW20 0EX, Surrey, England.
[Loreau, Michel] CNRS, Ctr Biodivers Theory & Modelling, Stn Ecol Expt, F-09200 Moulis, France.
[Mereu, Simone] Univ Sassari, Dept Sci Nat & Nat Resources, I-07100 Sassari, Italy.
[Mereu, Simone] Euromediterranean Ctr Climate Change CMCC, Impacts Agr Forest & Nat Ecosyst, Lecce, Italy.
[Messier, Christian] Univ Quebec Outaouais, Inst Sci Foret Tempere ISFORT, Ripon, PQ J0V 1V0, Canada.
[Muys, Bart] Katholieke Univ Leuven, Dept Earth & Environm Sci, Div Forest Nat & Landscape, B-3001 Louvain, Belgium.
[Nolet, Philippe] Univ Quebec Outaouais, Dept Nat Sci, Ripon, PQ J0V 1V0, Canada.
[Parker, John; Potvin, Catherine] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Perring, Mike] Univ Western Australia, Ecosyst Restorat & Intervent Ecol Res Grp, Sch Plant Biol, Crawley, WA 6009, Australia.
[Ponette, Quentin] Catholic Univ Louvain, Earth & Life Inst, Environm Sci, B-1348 Louvain La Neuve, Belgium.
[Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Reich, Peter] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
[Reich, Peter] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2753, Australia.
[Smith, Andy] Bangor Univ, Sch Environm Nat Resources & Geog, Bangor LL57 2UW, Gwynedd, Wales.
[Weih, Martin] Swedish Univ Agr Sci, Dept Crop Prod Ecol, S-75007 Uppsala, Sweden.
RP Verheyen, K (reprint author), Univ Ghent, Dept Forest & Water Management, Forest & Nat Lab, Geraardsbergsesteenweg 267, B-9090 Melle Gontrode, Belgium.
EM kris.verheyen@ugent.be; margot.vanhellemont@ugent.be;
harald.auge@ufz.de; lander.baeten@ugent.be; chris.baraloto@ecofog.gf;
nadia.barsoum@forestry.gsi.gov.uk; simonbgauthier@yahoo.ca;
helge.bruelheide@botanik.uni-halle.de;
bastien.castagneyrol@pierroton.inra.fr; douglas.godbold@boku.ac.at;
josephine.haase@biologie.uni-freiburg.de; andrew.hector@plants.ox.ac.uk;
herve.jactel@pierroton.inra.fr; julia.koricheva@rhul.ac.uk;
michel.loreau@ecoex-moulis.cnrs.fr; simonemereu@uniss.it;
messier.christian@uqam.ca; bart.muys@ees.kuleuven.be;
philippe.nole@uqo.ca; alain.paquette@gmail.com; parkerj@si.edu;
michael.perring@uwa.edu.au; quentin.ponette@uclouvain.be;
catherine.potvin@mcgill.ca; preich@umn.edu; a.r.smith@bangor.ac.uk;
martin.weih@slu.se; michael.scherer@biologie.uni-freiburg.de
RI Hector, Andrew/H-4199-2011; Smith, Andy/A-7512-2011; Koricheva, Julia
/G-6754-2011; Weih, Martin/H-5093-2011; Auge, Harald/D-4802-2015;
Parker, John/F-9761-2010;
OI Hector, Andrew/0000-0002-1309-7716; Smith, Andy/0000-0001-8580-278X;
Koricheva, Julia /0000-0002-9033-0171; Weih, Martin/0000-0003-3823-9183;
Auge, Harald/0000-0001-7432-8453; Parker, John/0000-0002-3632-7625;
Castagneyrol, Bastien/0000-0001-8795-7806
FU sDiv, the Synthesis Centre of the German Centre for Integrative
Biodiversity Research (iDiv) Halle-Jena-Leipzig [DFG FZT 118]
FX This paper is an outcome of a workshop kindly supported by sDiv, the
Synthesis Centre of the German Centre for Integrative Biodiversity
Research (iDiv) Halle-Jena-Leipzig (DFG FZT 118). The TreeDivNet
experiments could not have been established without the help and support
of many funding organizations and persons, too numerous to be listed
here individually.
NR 50
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U1 10
U2 56
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0044-7447
EI 1654-7209
J9 AMBIO
JI Ambio
PD FEB
PY 2016
VL 45
IS 1
BP 29
EP 41
DI 10.1007/s13280-015-0685-1
PG 13
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DA8EV
UT WOS:000368038800003
PM 26264716
ER
PT J
AU Kepler, SO
Pelisoli, I
Koester, D
Ourique, G
Romero, AD
Reindl, N
Kleinman, SJ
Eisenstein, DJ
Valois, ADM
Amaral, LA
AF Kepler, S. O.
Pelisoli, I.
Koester, D.
Ourique, G.
Romero, A. D.
Reindl, N.
Kleinman, S. J.
Eisenstein, D. J.
Valois, A. D. M.
Amaral, L. A.
TI New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data
Release 12
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE catalogues; stars: magnetic field; subdwarfs; white dwarfs
ID EXTREMELY LOW-MASS; OSCILLATION SPECTROSCOPIC SURVEY; CETI INSTABILITY
STRIP; 1ST DATA RELEASE; ATMOSPHERIC PARAMETERS; SDSS-III; SPECTRAL
CLASSIFICATION; EVOLUTIONARY SEQUENCES; METALLICITY DEPENDENCE;
LUMINOSITY FUNCTION
AB We report the discovery of 6576 new spectroscopically confirmed white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12. We obtain T-eff, log g and mass for hydrogen atmosphere white dwarf stars (DAs) and helium atmosphere white dwarf stars (DBs), estimate the calcium/helium abundances for the white dwarf stars with metallic lines (DZs) and carbon/helium for carbon-dominated spectra (DQs). We found one central star of a planetary nebula, one ultracompact helium binary (AM CVn), one oxygen line-dominated white dwarf, 15 hot DO/PG1159s, 12 new cataclysmic variables, 36 magnetic white dwarf stars, 54 DQs, 115 helium-dominated white dwarfs, 148 white dwarf + main-sequence star binaries, 236 metal-polluted white dwarfs, 300 continuum spectra DCs, 230 hot subdwarfs, 2936 new hydrogen-dominated white dwarf stars, and 2675 cool hydrogen-dominated subdwarf stars. We calculate the mass distribution of all 5883 DAs with S/N >= 15 in DR12, including the ones in DR7 and DR10, with an average S/N = 26, corrected to the 3D convection scale, and also the distribution after correcting for the observed volume, using 1/Vmax.
C1 [Kepler, S. O.; Pelisoli, I.; Ourique, G.; Romero, A. D.; Valois, A. D. M.; Amaral, L. A.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil.
[Koester, D.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Reindl, N.] Eberhard Karls Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Kleinman, S. J.] Gemini Observ, Hilo, HI 96720 USA.
[Eisenstein, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kepler, SO (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, BR-91501900 Porto Alegre, RS, Brazil.
EM kepler@if.ufrgs.br; ingrid.pelisoli@gmail.com;
koester@astrophysik.uni-kiel.de
RI Pelisoli, Ingrid/H-8619-2014; Romero, Alejandra/G-1644-2016; Kepler, S.
O. /H-5901-2012
OI Kepler, S. O. /0000-0002-7470-5703
FU CNPq-Brazil; MCIT/MEC-Brazil; German Aerospace Center (DLR) [05 OR
1507]; Alfred P. Sloan Foundation; National Science Foundation; US
Department of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX SOK, IP, GO, ADR, and ADMV are supported by CNPq-Brazil. DK received
support from programme Science without Borders, MCIT/MEC-Brazil. NR is
supported by the German Aerospace Center (DLR, grant 05 OR 1507). This
research has made use of NASA's Astrophysics Data System.; Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the US
Department of Energy Office of Science. The SDSS-III website is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, Carnegie Mellon
University, University of Florida, the French Participation Group, the
German Participation Group, Harvard University, the Instituto de
Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University.
NR 104
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 1
PY 2016
VL 455
IS 4
BP 3413
EP 3423
DI 10.1093/mnras/stv2526
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UH
UT WOS:000368009300001
ER
PT J
AU Shara, MM
Mikolajewska, J
Caldwell, N
Ilkiewicz, K
Drozd, K
Zurek, D
AF Shara, Michael M.
Mikolajewska, Joanna
Caldwell, Nelson
Ilkiewicz, Krystian
Drozd, Katarzyna
Zurek, David
TI The first transition Wolf-Rayet WN/C star in M31
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; binaries: symbiotic; stars: Wolf-Rayet
ID LARGE-MAGELLANIC-CLOUD; MASSIVE STARS; WR STARS; ANDROMEDA GALAXY; I.;
CLASSIFICATION; SPECTROSCOPY; BINARIES; CATALOG
AB Three decades of searches have revealed 154 Wolf-Rayet (WR) stars in M31, with 62 of WC type, 92 of WN type and zero of transition-type WN/C or WC/N. In apparent contrast, about two per cent of the WR stars in the Galaxy, the LMC and M33 simultaneously display strong lines of carbon and nitrogen, i.e. they are transition-type WN/C or WC/N stars. We report here the serendipitous discovery of M31 WR 84-1, the first transition star in M31, located at RA = 00(h)43(m)43(s).61 Dec. = +41 degrees 45'27".95 (J2000). We present its spectrum, classify it as WN5/WC6, and compare it with other known transition stars. The star is unresolved in Hubble Space Telescope narrow-band and broad-band images, while its spectrum displays strong, narrow emission lines of hydrogen, [N II], [S II] and [O III]; this indicates a nebula surrounding the star. The radial velocity of the nebular lines is consistent with that of gas at the same position in the disc of M31. The metallicity at the 11.8 kpc galactocentric distance of M31 WR 84-1 is approximately solar, consistent with other known transition stars. We suggest that modest numbers of reddened WR stars remain to be found in M31.
C1 [Shara, Michael M.; Zurek, David] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Mikolajewska, Joanna; Ilkiewicz, Krystian; Drozd, Katarzyna] N Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Shara, MM (reprint author), Amer Museum Nat Hist, Dept Astrophys, Cent Pk West,79th St, New York, NY 10024 USA.
EM mshara@amnh.org
FU Polish NCN [DEC-2013/10/M/ST9/00086]; NASA [NAS 5-26555]
FX This study has been supported in part by the Polish NCN grant
DEC-2013/10/M/ST9/00086. We gratefully acknowledge the fine support at
the MMT Observatory, and The Local Group Galaxy Survey conducted at NOAO
by Phil Massey and collaborators.; This research has made use of the
VizieR catalogue access tool, operated at CDS, Strasbourg, France. Based
on observations made with the NASA/ESA Hubble Space Telescope, obtained
from the Data Archive at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555.
NR 30
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 1
PY 2016
VL 455
IS 4
BP 3453
EP 3457
DI 10.1093/mnras/stv2455
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UH
UT WOS:000368009300005
ER
PT J
AU Hardcastle, MJ
Lenc, E
Birkinshaw, M
Croston, JH
Goodger, JL
Marshall, HL
Perlman, ES
Siemiginowska, A
Stawarz, L
Worrall, DM
AF Hardcastle, M. J.
Lenc, E.
Birkinshaw, M.
Croston, J. H.
Goodger, J. L.
Marshall, H. L.
Perlman, E. S.
Siemiginowska, A.
Stawarz, L.
Worrall, D. M.
TI Deep Chandra observations of Pictor A
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: individual: Pictor A; galaxies: jets; X-rays: galaxies
ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; RADIO GALAXY PICTOR; LARGE-SCALE
JETS; HOT-SPOTS; PARTICLE-ACCELERATION; M87 JET; CLUSTER ENVIRONMENTS;
RELATIVISTIC JETS; PKS 0637-752
AB We report on deep Chandra observations of the nearby broad-line radio galaxy Pictor A, which we combine with new Australia Telescope Compact Array (ATCA) observations. The new X-ray data have a factor of 4 more exposure than observations previously presented and span a 15 yr time baseline, allowing a detailed study of the spatial, temporal and spectral properties of the AGN, jet, hotspot and lobes. We present evidence for further time variation of the jet, though the flare that we reported in previous work remains the most significantly detected time-varying feature. We also confirm previous tentative evidence for a faint counterjet. Based on the radio through X-ray spectrum of the jet and its detailed spatial structure, and on the properties of the counterjet, we argue that inverse-Compton models can be conclusively rejected, and propose that the X-ray emission from the jet is synchrotron emission from particles accelerated in the boundary layer of a relativistic jet. For the first time, we find evidence that the bright western hotspot is also time-varying in X-rays, and we connect this to the small-scale structure in the hotspot seen in high-resolution radio observations. The new data allow us to confirm that the spectrum of the lobes is in good agreement with the predictions of an inverse-Compton model and we show that the data favour models in which the filaments seen in the radio images are predominantly the result of spatial variation of magnetic fields in the presence of a relatively uniform electron distribution.
C1 [Hardcastle, M. J.; Goodger, J. L.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Lenc, E.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia.
[Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Croston, J. H.] Univ Cambridge, Inst Continuing Educ, Cambridge CB23 8AQ, England.
[Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
EM m.j.hardcastle@herts.ac.uk
OI Lenc, Emil/0000-0002-9994-1593; Hardcastle, Martin/0000-0003-4223-1117
FU Commonwealth of Australia; Australian Research Council Centre of
Excellence [CE110001020]; UK STFC [ST/M001008/1, ST/M001326/1]; Polish
NSC [DEC-2012/04/A/ST9/00083]
FX We thank Rick Perley for providing radio images from Perley et al.
(1997), Dan Schwartz and Dan Harris for helpful comments on an earlier
draft of the paper, and the referee, Robert Laing, for numerous valuable
comments on the content and presentation. This research has made use of
data obtained from the Chandra Data Archive, and software provided by
the Chandra X-ray Center (CXC) in the application packages CIAO and
SHERPA. The Australia Telescope Compact Array is part of the Australia
Telescope National Facility which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. This research made use of ASTROPY, a
community-developed core PYTHON package for astronomy (Astropy
Collaboration 2013) hosted at http://www.astropy.org, and of APLPY, an
open-source plotting package for PYTHON hosted at
http://aplpy.github.com. The Centre for All-sky Astrophysics (CAASTRO)
is an Australian Research Council Centre of Excellence, funded by grant
CE110001020. MJH, JLG and JHC acknowledge support from the UK STFC via
grants ST/M001008/1 and ST/M001326/1. LS was supported by Polish NSC
grant DEC-2012/04/A/ST9/00083.
NR 92
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U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB 1
PY 2016
VL 455
IS 4
BP 3526
EP 3545
DI 10.1093/mnras/stv2553
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7UH
UT WOS:000368009300010
ER
PT J
AU Papacostas, KJ
Freestone, AL
AF Papacostas, Katherine J.
Freestone, Amy L.
TI Latitudinal gradient in niche breadth of brachyuran crabs
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Body size; brachyuran crab; diet; gut content analysis; latitude; niche
breadth; phylogenetic relatedness; range size
ID SPECIES RICHNESS GRADIENT; RANGE LIMITS; DIVERSITY GRADIENT; BODY-SIZE;
PHYLOGENETIC ANALYSIS; GEOGRAPHICAL RANGE; HOST-SPECIFICITY; MARINE;
SPECIALIZATION; TROPICS
AB AimNiche breadth has long been hypothesized to decrease at low latitudes and contribute to global patterns of species diversity. Range size, phylogenetic relatedness and body size also have hypothesized relationships with both latitude and niche breadth, which may further affect niche breadth patterns. Existing terrestrial data are inconclusive and few data exist on latitudinal gradients in niche breadth in the marine realm. We tested the latitude-niche breadth relationship in a marine system while exploring the correlations of both variables with range size, and accounting for relatedness and body size.
LocationGlobal.
MethodsWe compiled a global dataset on the dietary niche breadth of 39 brachyuran crab species from existing studies and additional analyses on species collected in Connecticut and Florida, USA and Bocas del Toro, Panama. Estimates of latitude, range size, clade and body size were obtained for each species. We then tested for correlations among focal variables and examined the strength of their relationships with diet breadth.
ResultsLatitude was the strongest predictor of niche breadth in temperate species, and the latitude-niche breadth relationship was stronger in larger-bodied species. The strongest predictor of the niche breadth of tropical species was clade, with the newest clade having the narrowest diet. Niche breadth was related to range size for both temperate and tropical species. Tropical species had larger ranges on average than temperate species.
Main conclusionsWe found an interesting division in the niche breadth relationships of temperate and tropical species; diets of temperate species were positively correlated with latitude, range size and body size, and diets of tropical species were related to range size and clade. Therefore, only temperate species demonstrated the predicted positive relationship between niche breadth and latitude, while evolutionary history was a stronger predictor of niche breadth in tropical species.
C1 [Papacostas, Katherine J.; Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA.
[Papacostas, Katherine J.] Conservat Int, Moore Ctr Sci & Oceans, Arlington, VA 22202 USA.
[Freestone, Amy L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Papacostas, KJ (reprint author), Temple Univ, Dept Biol, Philadelphia, PA 19122 USA.
EM kpapacostas@temple.edu
FU Smithsonian/Link Foundation fellowship programme (Smithsonian Marine
Station Contribution at Fort Pierce, Florida) [1002]; Quebec-Labrador
Foundation's Sounds Conservancy Grant; National Science Foundation
[0841377]; Division of Ocean Sciences [1225583]
FX We thank C. Clark, J. Hoffman and M. Vaca for assistance with data
entry, the Smithsonian Tropical Research Institute's Bocas del Toro
Research Station and the Smithsonian Marine Station for use of their
facilities for subtropical and tropical crab collections, Z.
Mckie-Krisberg and A. Durkin for coding assistance, E. Cordes, R.
Sanders, B. Sewall and P. Petraitis for useful feedback during the
development of the project, and J. Belmaker as well as three anonymous
reviewers. This study was supported by the Smithsonian/Link Foundation
fellowship programme (Smithsonian Marine Station Contribution at Fort
Pierce, Florida, no. 1002), the Quebec-Labrador Foundation's Sounds
Conservancy Grant, and the National Science Foundation through both the
Graduate STEM Fellows in K-12 Education programme under grant no.
0841377 and the Division of Ocean Sciences under grant no. 1225583. Any
opinion, findings, conclusions or recommendations expressed in this
material are those of the authors, do not necessarily reflect the
position of the National Science Foundation and no official endorsement
should be inferred.
NR 57
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U1 4
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1466-822X
EI 1466-8238
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD FEB
PY 2016
VL 25
IS 2
BP 207
EP 217
DI 10.1111/geb.12400
PG 11
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA DA3VY
UT WOS:000367729100008
ER
PT J
AU Holmquist, JR
Finkelstein, SA
Garneau, M
Massa, C
Yu, ZC
MacDonald, GM
AF Holmquist, James R.
Finkelstein, Sarah A.
Garneau, Michelle
Massa, Charly
Yu, Zicheng
MacDonald, Glen M.
TI A comparison of radiocarbon ages derived from bulk peat and selected
plant macrofossils in basal peat cores from circum-arctic peatlands
SO QUATERNARY GEOCHRONOLOGY
LA English
DT Article
DE Peatland; Radiocarbon; Holocene; Basal peat dating
ID CARBON ACCUMULATION; DIFFERENT FRACTIONS; HOLOCENE CLIMATE; CANADA;
SAMPLES; QUEBEC; ALASKA; RECONSTRUCTION; AMS
AB Databases of basal radiocarbon (C-14) ages from peatlands have been used extensively at regional and global scales to examine peatland initiation, land-cover change and carbon cycle dynamics. Many dates collected and analyzed before the 1990s are from bulk peat samples of organic-rich sediments, and such basal radiocarbon ages might have been either too young or too old due to inclusion of non-contemporary carbon via translocation from higher horizons. However, there is rarely a systematic assessment of this problem, especially for large datasets. Here we used AMS C-14 dating of both bulk peat and individual macrofossils from the same basal horizon at each of 40 peatland cores across North America and Siberia to evaluate the differences between the two sample types. Our results show that there is no significant or systematic difference between ages derived from bulk material and plant macrofossils. We find that the greatest age overlap of 2 sigma calibrated age distributions occurred between bulk peat and aboveground macrofossils such as moss fragments, seeds, and herbaceous leaves, suggesting that the bulk material is contemporaneous with the aboveground biomass and active carbon uptake. Dates including wood fragments showed wider divergence compared to moss fragments, seeds, and leaves. We find no evidence for statistically significant and consistent bias introduced by C-14 dating of bulk basal peat. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Holmquist, James R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Finkelstein, Sarah A.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 1A1, Canada.
[Garneau, Michelle] Univ Quebec Montreal UQAM, Dept Geog, Montreal, PQ, Canada.
[Garneau, Michelle] Univ Quebec Montreal UQAM, GEOTOP, Montreal, PQ, Canada.
[Yu, Zicheng] Lehigh Univ, Earth & Environm Sci Dept, Bethlehem, PA USA.
[MacDonald, Glen M.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
[Massa, Charly] Univ Hawaii Manoa, Dept Geog, Honolulu, HI 96822 USA.
RP Holmquist, JR (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM HolmquistJ@si.edu
RI Finkelstein, Sarah/K-8202-2012; Yu, Zicheng/D-4108-2012
OI Finkelstein, Sarah/0000-0002-8239-399X;
FU NSF [NSF-0843685, NSF-0628598, EAR-0819717, ARC-1107981]; Ontario
Ministry of Natural Resources Far North Branch; Natural Sciences and
Engineering Research Council of Canada (NSERC); Ontario Ministry of the
Environment through the Climate Change and Multiple Stressor Research
Program at Laurentian University; Natural Sciences and Engineering
Research Council of Canada [NSERC-RDCPJ365867-8]; [IPY-2006-SR1-CC-096]
FX NSF (NSF-0843685; NSF-0628598) supported dates reported by Holmquist et
al. (2014), MacDonald (Unpublished), as well as additional bulk-peat AMS
14C dates. The Ontario Ministry of Natural Resources Far
North Branch, Natural Sciences and Engineering Research Council of
Canada (NSERC), and the Ontario Ministry of the Environment through the
Climate Change and Multiple Stressor Research Program at Laurentian
University funded dates from sites reported by Finkelstein.
IPY-2006-SR1-CC-096 project and Natural Sciences and Engineering
Research Council of Canada (NSERC-RDCPJ365867-8) supported dates
reported by Gameau. NSF (EAR-0819717; ARC-1107981) supported dates
reported by Yu. The authors would like to thank Dave Beilman, Katherine
Willis, LeeAnn Fishback and the staff at the Churchill Northern Studies
Centre for field collections of the cores with the pre-fix JBL and CH.
DeBeers Canada provided logistical support for research out of Victor
Mine, in northern Ontario. The authors would also like to thank K.
Cleary and J. Loisel, J. McLaughlin, B. Hamel, M. Packalen, B. O'Reilly,
C. Friel, J. Bunbury and J. Devlin for field and lab assistance. We also
acknowledge the contributions of three anonymous reviewers whose
feedback greatly improved this manuscript.
NR 37
TC 2
Z9 2
U1 3
U2 11
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1871-1014
EI 1878-0350
J9 QUAT GEOCHRONOL
JI Quat. Geochronol.
PD FEB
PY 2016
VL 31
BP 53
EP 61
DI 10.1016/j.quageo.2015.10.003
PG 9
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA CZ9JH
UT WOS:000367413400007
ER
PT J
AU Aira, M
Olcina, J
Perez-Losada, M
Dominguez, J
AF Aira, Manuel
Olcina, Jessica
Perez-Losada, Marcos
Dominguez, Jorge
TI Characterization of the bacterial communities of casts from Eisenia
andrei fed with different substrates
SO APPLIED SOIL ECOLOGY
LA English
DT Article
DE Bacterial communities; Bacterial diversity; Bar-coded pyrosequencing;
Earthworms; Eisenia andrei; Decomposition
ID EARTHWORM LUMBRICUS-RUBELLUS; MICROBIAL COMMUNITIES; FOETIDA
OLIGOCHAETA; SOIL; DIVERSITY; GUT; VERMICOMPOSTS; INTESTINE; SEQUENCES;
PROFILES
AB Earthworms play a key role during the first stage of decomposition by enhancing the activity of microorganisms. As organic matter passes throughout the earthworm gut, nutrient pools and microbial communities are modified and released in casts. Here we used 16S rRNA pyrosequencing and metagenomic analysis to characterize the bacterial communities of casts from the earthworm Eisenia andrei fed with different food sources (cow, horse and pig manure). We found that the bacterial communities of cast strongly depended on the food source ingested by earthworms; although, no differences in a-diversity were detected. Bacterial communities of casts were mainly comprised of a variable amount of OTUs (operational taxonomic unit) belonging to the phyla Proteobacteria, Firmicutes, Actinobacteria and Bacteroidetes, with minor contributions from the phyla Verrucomicrobia, Chloroflexi, Hydrogenedentes, Latescibacteria, Planctomycetes and Candidatus Saccharibacteria. From these bacterial profiles we found OTUs that worked out as biomarkers for each bacterial community allowing us to discriminate among food sources. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Aira, Manuel; Olcina, Jessica; Dominguez, Jorge] Univ Vigo, Dept Ecol & Biol Anim, E-36310 Vigo, Spain.
[Perez-Losada, Marcos] Univ Porto, CIBIO InBIO, Ctr Invest Biodiversidade & Recursos Genet, P-4485661 Vairao, Portugal.
[Perez-Losada, Marcos] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA.
[Perez-Losada, Marcos] Smithsonian Inst, US Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP Aira, M (reprint author), Fac Ciencias, Dept Ecol & Biol Anim, Campus Univ As Lagoas, E-32004 Orense, Spain.
EM aira@uvigo.es
RI Aira, Manuel/B-4506-2016; Perez-Losada, Marcos/I-4407-2013
OI Aira, Manuel/0000-0002-2513-4609; Perez-Losada,
Marcos/0000-0002-2585-4657
FU Ministerio de Economia y Competitividad [CTM2013-42540-R]; Xunta de
Galicia [CN2012/305]
FX This study was supported by grants from the Ministerio de Economia y
Competitividad (CTM2013-42540-R) and the Xunta de Galicia (CN2012/305)
NR 48
TC 1
Z9 1
U1 12
U2 59
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0929-1393
EI 1873-0272
J9 APPL SOIL ECOL
JI Appl. Soil Ecol.
PD FEB
PY 2016
VL 98
BP 103
EP 111
DI 10.1016/j.apsoil.2015.10.002
PG 9
WC Soil Science
SC Agriculture
GA CX9AW
UT WOS:000365998100012
ER
PT J
AU Attaran-Farimani, G
Estekani, S
Springer, VG
Crimmen, O
Johnson, GD
Baldwin, CC
AF Attaran-Farimani, Gilan
Estekani, Sanaz
Springer, Victor G.
Crimmen, Oliver
Johnson, G. David
Baldwin, Carole C.
TI Validation of the synonymy of the teleost blenniid fish species Salarias
phantasticus Boulenger 1897 and Salarias anomalus Regan 1905 with
Ecsenius pulcher (Murray 1887) based on DNA barcoding and morphology
SO ZOOTAXA
LA English
DT Article
DE Blenniidae; taxonomy; Color polymorphism; Oman Sea; Iran; Integrative
taxonomy; Parasitic crustacean; Blenniid sex anatomy
ID TRIPTERYGIIDAE; SEQUENCES; GOBIIDAE; REVEALS; GENES
AB As currently recognized, Ecsenius pulcher includes Salarias pulcher (type material has a banded color pattern), S. anomalus (non-banded), and S. phantasticus (banded). The color patterns are not sex linked, and no other morphological features apparently distinguish the three nominal species. The recent collection of banded and non-banded specimens of Ecsenius pulcher from Iran has provided the first tissue samples for genetic analyses. Here we review the taxonomic history of E. pulcher and its included synonyms and genetically analyze tissue samples of both color patterns. Salarias anomalus is retained as a synonym of E. pulcher because DNA barcode data suggest that they represent banded and non-banded color morphs of a single species. Furthermore, the large size of the largest type specimen of S. anomalus (herein designated as the lectotype) suggests that it belongs to E. pulcher. A single non-banded specimen from Iran is genetically distinct from E. pulcher and appears to represent an undescribed species. Salarias phantasticus is retained as a synonym of E. pulcher because the primary morphological difference between the two nominal species-presence of spots on the dorsal fin in E. pulcher and absence of those spots in S. phantasticus-is not a valid taxonomic character; rather, the spots represent galls that contain the larval stages of a parasitic crustacean. As males and females of Ecsenius species have been confused in the literature, we describe and illustrate the genital regions of both and comment on possible new blenniid synapomorphies that our investigation revealed.
C1 [Attaran-Farimani, Gilan; Estekani, Sanaz] Chabahar Maritime Univ, Fac Marine Sci, Chabahar, Iran.
[Springer, Victor G.; Johnson, G. David; Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Crimmen, Oliver] Nat Hist Museum, London, England.
RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM baldwinc@si.edu
NR 42
TC 0
Z9 0
U1 1
U2 4
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 29
PY 2016
VL 4072
IS 2
BP 171
EP 184
PG 14
WC Zoology
SC Zoology
GA DC7HG
UT WOS:000369389800002
PM 27395917
ER
PT J
AU Chang, D
Duda, TF
AF Chang, Dan
Duda, Thomas F., Jr.
TI Age-related association of venom gene expression and diet of predatory
gastropods
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
DE Conus; Conotoxin; Developmental plasticity; Predator-prey interactions
ID ONTOGENIC CHANGE; MATHEMATICAL-THEORY; MARINE GASTROPODS; RAPID
EVOLUTION; CONUS-EBRAEUS; TOXIN GENES; PREY; POPULATIONS; DIVERSITY;
ECOLOGY
AB Background: Venomous organisms serve as wonderful systems to study the evolution and expression of genes that are directly associated with prey capture. To evaluate the relationship between venom gene expression and prey utilization, we examined these features among individuals of different ages of the venomous, worm-eating marine snail Conus ebraeus. We determined expression levels of six genes that encode venom components, used a DNA-based approach to evaluate the identity of prey items, and compared patterns of venom gene expression and dietary specialization.
Results: C. ebraeus exhibits two major shifts in diet with age-an initial transition from a relatively broad dietary breadth to a narrower one and then a return to a broader diet. Venom gene expression patterns also change with growth. All six venom genes are up-regulated in small individuals, down-regulated in medium-sized individuals, and then either up-regulated or continued to be down-regulated in members of the largest size class. Venom gene expression is not significantly different among individuals consuming different types of prey, but instead is coupled and slightly delayed with shifts in prey diversity.
Conclusion: These results imply that changes in gene expression contribute to intraspecific variation of venom composition and that gene expression patterns respond to changes in the diversity of food resources during different growth stages.
C1 [Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
[Chang, Dan] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA.
[Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Chang, Dan] Univ Calif Santa Cruz, 1156 High St,Mail Stop EEBiol, Santa Cruz, CA 95064 USA.
RP Chang, D (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.; Chang, D (reprint author), Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.; Chang, D (reprint author), Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA.
FU University of Michigan Museum of Zoology
FX We thank Alex Kerr, Susanne Wilkins, Marielle Terbio, Carmen Kautz and
Kirstie Goodman-Randall at University of Guam Marine Lab for their
assistance with field collections. We acknowledge Jincong Tao in the
Molecular Core Lab at University of Michigan School of Dentistry for his
help with the Real-time PCR. We thank the Department of Fishery and
Wildlife Sciences at Guam for issuing collection permits and the US Fish
and Wildlife Service for processing the specimen importation from a US
Territory. This project was funded by two Hinsdale-Walker Fellowships
awarded to D.C. by the University of Michigan Museum of Zoology.
NR 76
TC 0
Z9 0
U1 2
U2 4
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD JAN 28
PY 2016
VL 16
AR 27
DI 10.1186/s12862-016-0592-5
PG 12
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA DC4BG
UT WOS:000369164100001
PM 26818019
ER
PT J
AU Rushing, CS
Ryder, TB
Marra, PP
AF Rushing, Clark S.
Ryder, Thomas B.
Marra, Peter P.
TI Quantifying drivers of population dynamics for a migratory bird
throughout the annual cycle
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE climate change; habitat loss; migratory connectivity; population
dynamics; population limitation; seasonal interactions
ID UNITED-STATES; CONSERVATION; SONGBIRD; IMPACT; ABUNDANCE; CLIMATE;
MARKERS; RANGES; MODELS
AB Worldwide, migratory species are undergoing rapid declines but understanding the factors driving these declines is hindered by missing information about migratory connectivity and the lack of data to quantify environmental processes across the annual cycle. Here, we combined range-wide information about migratory connectivity with global remote-sensing data to quantify the relative importance of breeding and non-breeding environmental processes to persistent long-term population declines of a migratory songbird, the wood thrush (Hylocichla mustelina). Consistent with theoretical predictions about population limitation of migratory birds, our results suggest that habitat loss and climate have contributed to the observed declines in wood thrush breeding abundance, yet the relative importance of breeding versus non-breeding factors is population-specific. For example, high-abundance core breeding populations appear to be more limited by habitat loss, whereas low-abundance, peripheral populations appear to be limited by climate-driven seasonal interactions. Further, our analysis indicates that the relative impact of breeding habitat loss is at least three to six times greater than the impact of equivalent nonbreeding habitat loss and therefore the steepest regional declines have likely been driven by the loss of breeding habitat. These results underscore the need for population-specific conservation strategies implemented throughout the annual cycle to reverse long-term declines.
C1 [Rushing, Clark S.; Ryder, Thomas B.; Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
RP Rushing, CS (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
EM rushingc@si.edu
FU Smithsonian Institution; US Fish and Wildlife Service; Strategic
Environmental Research and Development Program
FX C.S.R. was supported by a James Smithson and a Didden Postdoctoral
fellowship from the Smithsonian Institution. Funding was provided by US
Fish and Wildlife Service and the Strategic Environmental Research and
Development Program.
NR 50
TC 4
Z9 5
U1 6
U2 20
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD JAN 27
PY 2016
VL 283
IS 1823
AR 20152846
DI 10.1098/rspb.2015.2846
PG 10
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DL7ZH
UT WOS:000375858400001
ER
PT J
AU Temeles, EJ
Newman, JT
Newman, JH
Cho, SY
Mazzotta, AR
Kress, WJ
AF Temeles, Ethan J.
Newman, Julia T.
Newman, Jennifer H.
Cho, Se Yeon
Mazzotta, Alexandra R.
Kress, W. John
TI Pollinator Competition as a Driver of Floral Divergence: An Experimental
Test
SO PLOS ONE
LA English
DT Article
ID FLOWER COLOR POLYMORPHISM; PURPLE-THROATED CARIBS; DEEP COROLLA TUBES;
TROPICAL HUMMINGBIRD; RESOURCE COMPETITION; MEDIATED SELECTION;
EULAMPIS-JUGULARIS; LONG TONGUES; POPULATIONS; BUMBLEBEES
AB Optimal foraging models of floral divergence predict that competition between two different types of pollinators will result in partitioning, increased assortative mating, and divergence of two floral phenotypes. We tested these predictions in a tropical plant-pollinator system using sexes of purple-throated carib hummingbirds (Anthracothorax jugularis) as the pollinators, red and yellow inflorescence morphs of Heliconia caribaea as the plants, and fluorescent dyes as pollen analogs in an enclosed outdoor garden. When foraging alone, males exhibited a significant preference for the yellow morph of H. caribaea, whereas females exhibited no preference. In competition, males maintained their preference for the yellow morph and through aggression caused females to over-visit the red morph, resulting in resource partitioning. Competition significantly increased within-morph dye transfer (assortative mating) relative to non-competitive environments. Competition and partitioning of color morphs by sexes of purple-throated caribs also resulted in selection for floral divergence as measured by dye deposition on stigmas. Red and yellow morphs did not differ significantly in dye deposition in the competition trials, but differences in dye deposition and preferences for morphs when sexes of purple-throated caribs foraged alone implied fixation of one or the other color morph in the absence of competition. Competition also resulted in selection for divergence in corolla length, with the red morph experiencing directional selection for longer corollas and the yellow morph experiencing stabilizing selection on corolla length. Our results thus support predictions of foraging models of floral divergence and indicate that pollinator competition is a viable mechanism for divergence in floral traits of plants.
C1 [Temeles, Ethan J.; Newman, Julia T.; Newman, Jennifer H.; Cho, Se Yeon; Mazzotta, Alexandra R.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA.
[Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20560 USA.
RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA.
EM ejtemeles@amherst.edu
FU Amherst College; Smithsonian Institution; National Science Foundation
[DEB-614218, DEB-1353783]
FX This research was supported by awards from Amherst College
(www.amherst.edu), The Smithsonian Institution (www.si.edu), and the
National Science Foundation (www.nsf.gov) grants DEB-614218 and
DEB-1353783. The funders had no role in the study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 53
TC 0
Z9 0
U1 13
U2 34
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JAN 27
PY 2016
VL 11
IS 1
AR e0146431
DI 10.1371/journal.pone.0146431
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC9GD
UT WOS:000369528200014
PM 26814810
ER
PT J
AU Winston, JE
AF Winston, Judith E.
TI Bryozoa of Floridan Oculina reefs
SO ZOOTAXA
LA English
DT Article
DE Bryozoa; Cheilostomata; Cribrilinidae; Cyclostomata; Oculina varicosa;
Scleractinia; deepwater corals; Florida
ID VARICOSA CORAL REEFS; CHEILOSTOME BRYOZOA; MARINE BRYOZOA; BRAZIL;
WATER; CYCLOSTOMATA; REVISION; SHELF
AB The deep-water Oculina coral reefs on the continental shelf off the east central coast of Florida are a unique protected marine habitat. A complete inventory of the Oculina-associated fauna is important to support its conservation. This paper provides an inventory of the bryozoans of the Oculina reef area. Unusually, the bryozoan fauna is dominated by encrusting cribrilinid bryozoans. These include two new species of Puellina and three other Floridan-Atlantic shelf Puellina only recently described. Additional cribrilinid species belong to the genera Klugerella and Rosulapelta. Other bryozoans found in the habitat include 38 encrusting cheilostome species, six of them new to science, belonging to the genera Callopora, Parasmittina, Parasmittina, Smittina, Microporella and Stephanollona. Cyclostomes were only sparsely represented, comprising three encrusting taxa.
C1 [Winston, Judith E.] Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
RP Winston, JE (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM judithewinston@gmail.com
NR 130
TC 1
Z9 1
U1 0
U2 8
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 27
PY 2016
VL 4071
IS 1
BP 1
EP 81
PG 81
WC Zoology
SC Zoology
GA DC7GP
UT WOS:000369388000001
PM 27395907
ER
PT J
AU Ryder, TB
Sillett, TS
AF Ryder, Thomas B.
Sillett, T. Scott
TI Climate, demography and lek stability in an Amazonian bird
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE survival; recruitment; pipridae; lek stability; El Nino Southern
Oscillation
ID GROUSE TETRAO-TETRIX; MALE MATING SUCCESS; NINO SOUTHERN-OSCILLATION;
WIRE-TAILED MANAKIN; MALE SAGE GROUSE; SEXUAL SELECTION; LEKKING BIRD;
EL-NINO; FRUIT PRODUCTION; TROPICAL FOREST
AB Lekking is a rare, but iconic mating system where polygynous males aggregate and perform group displays to attract females. Existing theory postulates that demographic and environmental stability are required for lekking to be an evolutionarily viable reproductive strategy. However, we lack empirical tests for the hypotheses that lek stability is facilitated by age-specific variation in demographic rates, and by predictable, abundant resources. To address this knowledge gap, we use multistate models to examine how two demographic elements of lek stability-male survival and recruitment-vary with age, social status and phase of the El Nino Southern Oscillation (ENSO) in a Neotropical frugivorous bird, the wire-tailed manakin (Pipra filicauda). Our results show that demographic and environmental conditions were related to lek stability in the Ecuadorean Amazon. Apparent annual survival probability of territorial males was higher than that of non-territorial floaters, and recruitment probability increased as males progressed in an age-graded queue. Moreover, annual survival of territorial males and body condition of both floaters and territory holders were higher following years with El Nino conditions, associated with reduced rainfall and probably higher fruit production in the northern Neotropics, and lower after years with wet, La Nina conditions that predominated our study. Recruitment probabilities varied annually, independent of ENSO phase, and increased over our study period, but the annual mean number of territorial males per lek declined. Our results provide empirical support for hypothesized demographic and environmental drivers of lek dynamics. This study also suggests that climate-mediated changes in resource availability can affect demography and subsequent lek stability in a relatively buffered, lowland rainforest.
C1 [Ryder, Thomas B.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA.
RP Ryder, TB (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA.
EM rydert@si.edu
FU Harris World Ecology Center; National Science Foundation [IOB 0508189,
IOS 1353085]; Smithsonian Migratory Bird Center
FX This research was funded by the Harris World Ecology Center, National
Science Foundation (IOB 0508189 and IOS 1353085) and the Smithsonian
Migratory Bird Center.
NR 67
TC 1
Z9 1
U1 11
U2 26
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD JAN 27
PY 2016
VL 283
IS 1823
AR 20152314
DI 10.1098/rspb.2015.2314
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA DB3YC
UT WOS:000368448700008
ER
PT J
AU Hartmann, L
Mecke, S
Kieckbusch, M
Mader, F
Kaiser, H
AF Hartmann, Lukas
Mecke, Sven
Kieckbusch, Max
Mader, Felix
Kaiser, Hinrich
TI A new species of bent-toed gecko, genus Cyrtodactylus Gray, 1827
(Reptilia: Squamata: Gekkonidae), from Jawa Timur Province, Java,
Indonesia, with taxonomic remarks on C. fumosus (Muller, 1895)
SO ZOOTAXA
LA English
DT Article
DE Cyrtodactylus klakahensis sp nov.; C. fumosus; C. marmoratus;
Lacertilia; Gekkonidae; bent-toed geckos; East Java; Indonesia; Greater
Sunda Islands; morphology
ID MALAYSIA; ISLAND; SULAWESI; WEST; ARCHIPELAGO; PHYLOGENY; AUSTRALIA;
SAURIA; EAST
AB A new species of the gekkonid lizard genus Cyrtodactylus Gray, 1827 is described from Klakah, Lumajang Regency, Jawa Timur Province, Java, Indonesia. Cyrtodactylus klakahensis sp. nov. can be distinguished from all other congeners by the presence of (1) a deep precloacal groove in males, (2) three rows of enlarged precloacofemoral scales, of which the third row bears 37-38 pores in males, (3) three or four rows of enlarged scales between the precloacofemoral scale rows and the cloaca, forming distinct chevrons, (4) raised and strongly keeled dorsal tubercles in 15-19 rows at midbody, (5) an indistinct lateral fold, (6) 17-20 subdigital lamellae under the 4th toe, and (7) subcaudal scales which are not transversely enlarged. Cyrtodactylus klakahensis sp. nov. is only the third bent-toed gecko species described from Java, indicating that the diversity of this genus on this island has been neglected in the past. Furthermore, we confirm that C. fumosus (Muller, 1895) is a species that possesses a precloacal groove in males and is most likely restricted to northern Sulawesi. That species is defined by a single female holotype (NMB-REPT 2662). Specimens in museum collections catalogued as C. fumosus from localities elsewhere are misidentified and likely represent undescribed species.
C1 [Hartmann, Lukas; Mecke, Sven; Kieckbusch, Max] Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat, Karl von Frisch Str 8, D-35032 Marburg, Germany.
[Hartmann, Lukas; Mecke, Sven; Kieckbusch, Max] Univ Marburg, Fac Biol, Zool Collect Marburg, Karl von Frisch Str 8, D-35032 Marburg, Germany.
[Mader, Felix] Janusstr 5, D-93051 Regensburg, Germany.
[Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA.
[Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP Hartmann, L; Mecke, S (reprint author), Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat, Karl von Frisch Str 8, D-35032 Marburg, Germany.; Hartmann, L; Mecke, S (reprint author), Univ Marburg, Fac Biol, Zool Collect Marburg, Karl von Frisch Str 8, D-35032 Marburg, Germany.
EM hartmann.lukas@students.uni-marburg.de; meckes@staff.uni-marburg.de
FU AMNH collection study
FX The authors thank Gunther Kohler and Linda Acker (SMF), Denis Vallan and
Urs Wuest (NMB), Esther Dondorp (RMNH), Raffael Ernst and Markus Auer
(MTKD), Patrick Campbell (BMNH), Christopher J. Raxworthy, David A.
Kizirian, David A. Dickey, and Lauren Vonnahme (AMNH), Max Nickerson and
Kenneth Krysko (FLMNH), Joseph Martinez and Jose Rosado (MCZ), Kelvin
Lim (ZRC), and Frank Glaw (ZSM) for allowing examination of material in
their care. Furthermore, we are grateful to Linda Acker and Georg
Gassner (NHM) for providing some of the literature cited in the
reference section. Andre P. Koch (SNHMB) and Olivier Pauwels (IRSNB)
provided helpful reviews of the manuscript. This study was supported by
an AMNH collection study grant to SM.
NR 66
TC 6
Z9 6
U1 2
U2 4
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 26
PY 2016
VL 4067
IS 5
BP 552
EP 568
PG 17
WC Zoology
SC Zoology
GA DC7FT
UT WOS:000369385500002
PM 27395895
ER
PT J
AU Chesser, RT
AF Chesser, R. Terry
TI A replacement name for Asthenes wyatti perijanus Phelps 1977
SO ZOOTAXA
LA English
DT Editorial Material
ID FURNARIIDAE
C1 [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
RP Chesser, RT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 26
PY 2016
VL 4067
IS 5
BP 599
EP 599
PG 1
WC Zoology
SC Zoology
GA DC7FT
UT WOS:000369385500009
PM 27395902
ER
PT J
AU Smith, FA
Hammond, JI
Balk, MA
Elliott, SM
Lyons, SK
Pardi, MI
Tome, CP
Wagner, PJ
Westover, ML
AF Smith, Felisa A.
Hammond, John I.
Balk, Meghan A.
Elliott, Scott M.
Lyons, S. Kathleen
Pardi, Melissa I.
Tome, Catalina P.
Wagner, Peter J.
Westover, Marie L.
TI Exploring the influence of ancient and historic megaherbivore
extirpations on the global methane budget
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE trophic downgrading; megaherbivores; rinderpest; bison overkill;
Anthropocene
ID LATE QUATERNARY EXTINCTIONS; ATMOSPHERIC METHANE; ANTHROPOGENIC
EMISSIONS; NORTH-AMERICA; BODY-MASS; PLEISTOCENE; MAMMALS; VARIABILITY;
MEGAFAUNA; PLAINS
AB Globally, large-bodied wild mammals are in peril. Because "mega-mammals" have a disproportionate influence on vegetation, trophic interactions, and ecosystem function, declining populations are of considerable conservation concern. However, this is not new; trophic downgrading occurred in the past, including the African rinderpest epizootic of the 1890s, the massive Great Plains bison kill-off in the 1860s, and the terminal Pleistocene extinction of megafauna. Examining the consequences of these earlier events yields insights into contemporary ecosystem function. Here, we focus on changes inmethane emissions, produced as a byproduct of enteric fermentation by herbivores. Although methane is similar to 200 times less abundant than carbon dioxide in the atmosphere, the greater efficiency of methane in trapping radiation leads to a significant role in radiative forcing of climate. Using global datasets of late Quaternary mammals, domestic livestock, and human population from the United Nations as well as literature sources, we develop a series of allometric regressions relating mammal body mass to population density and CH4 production, which allows estimation of methane production by wild and domestic herbivores for each historic or ancient time period. We find the extirpation ofmegaherbivores reduced global enteric emissions between 2.2-69.6 Tg CH4 y(-1) during the various time periods, representing a decrease of 0.8-34.8% of the overall inputs to tropospheric input. Our analyses suggest that large-bodied mammals have a greater influence on methane emissions than previously appreciated and, further, that changes in the source pool from herbivores can influence global biogeochemical cycles and, potentially, climate.
C1 [Smith, Felisa A.; Hammond, John I.; Balk, Meghan A.; Pardi, Melissa I.; Tome, Catalina P.; Westover, Marie L.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Elliott, Scott M.] Los Alamos Natl Lab, Sea Ice Modeling, Ocean, Climate, POB 1663, Los Alamos, NM 87545 USA.
[Lyons, S. Kathleen; Wagner, Peter J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Smith, FA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
EM fasmith@unm.edu
FU National Institute of Biomedical Imaging and Bioengineering
[T32EB009414]; National Institute of General Medical Sciences
[K12GM088021]; National Science Foundation [BIO-0541625]
FX We thank S. Finnegan for providing crucial stimulus to actually pursue
the project. This research was originally inspired by National Public
Radio's Wait Wait Don't Tell Me news program. M.A.B. and M.I.P. were
fellows in the Program in Interdisciplinary Biological and Biomedical
Sciences at the University of New Mexico, supported by National
Institute of Biomedical Imaging and Bioengineering Grant T32EB009414 (to
F.A.S. and J.H. Brown, principal investigators); J.I.H. was supported by
National Institute of General Medical Sciences Grant K12GM088021. The
National Science Foundation provided financial support (Grant
BIO-0541625 to F.A.S., principal investigator, and S. K. Lyons and S. K.
M. Ernest, co-principal investigators).
NR 51
TC 1
Z9 1
U1 13
U2 29
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 26
PY 2016
VL 113
IS 4
BP 874
EP 879
DI 10.1073/pnas.1502547112
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DB6IJ
UT WOS:000368617900030
PM 26504225
ER
PT J
AU Zahid, HJ
Robinson, E
Kelly, RL
AF Zahid, H. Jabran
Robinson, Erick
Kelly, Robert L.
TI Agriculture, population growth, and statistical analysis of the
radiocarbon record
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE archeology; paleodemography; radiocarbon dating; hunter-gatherers;
agriculture
ID NEOLITHIC DEMOGRAPHIC-TRANSITION; MODERN HUMANS; CLIMATE-CHANGE;
NORTH-AMERICA; EUROPE; AGE; PLEISTOCENE; DATES; EXPANSIONS; AUSTRALIA
AB The human population has grown significantly since the onset of the Holocene about 12,000 y ago. Despite decades of research, the factors determining prehistoric population growth remain uncertain. Here, we examine measurements of the rate of growth of the prehistoric human population based on statistical analysis of the radiocarbon record. We find that, during most of the Holocene, human populations worldwide grew at a long-term annual rate of 0.04%. Statistical analysis of the radiocarbon record shows that transitioning farming societies experienced the same rate of growth as contemporaneous foraging societies. The same rate of growth measured for populations dwelling in a range of environments and practicing a variety of subsistence strategies suggests that the global climate and/or endogenous biological factors, not adaptability to local environment or subsistence practices, regulated the long-term growth of the human population during most of the Holocene. Our results demonstrate that statistical analyses of large ensembles of radiocarbon dates are robust and valuable for quantitatively investigating the demography of prehistoric human populations worldwide.
C1 [Zahid, H. Jabran] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Robinson, Erick; Kelly, Robert L.] Univ Wyoming, Dept Anthropol, Laramie, WY 82071 USA.
RP Zahid, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Robinson, E (reprint author), Univ Wyoming, Dept Anthropol, Laramie, WY 82071 USA.
EM zahid@cfa.harvard.edu; erick.robinson@uwyo.edu
FU Clay Postdoctoral Fellowship; [NSF-1418858]
FX We thank the anonymous reviewers for comments that significantly
improved the manuscript. We thank Ben Johnson and Anna Barnacka for
assistance in the statistical analysis, and Margaret Geller, Marc Vander
Linden, Megan Taddonio, Hugh Hudson, and Anna Barnacka for careful
reading of the manuscript. Mike Berry compiled the CO data. Nathaniel
Kitchel and Justin McKeel curated data supplied by the Wyoming State
Historic Preservation Office. H.J.Z. gratefully acknowledges the
generous support of the Clay Postdoctoral Fellowship and encouragement
from Margaret Geller. E.R. and R.L.K. are supported by NSF-1418858
(principal investigator, R.L.K.).
NR 47
TC 8
Z9 8
U1 8
U2 26
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 26
PY 2016
VL 113
IS 4
BP 931
EP 935
DI 10.1073/pnas.1517650112
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DB6IJ
UT WOS:000368617900039
PM 26699457
ER
PT J
AU Truelove, N
Behringer, DC
Butler, MJ
Preziosi, RF
AF Truelove, Nathan
Behringer, Donald C.
Butler, Mark J.
Preziosi, Richard F.
TI Isolation and characterization of eight polymorphic microsatellites for
the spotted spiny lobster, Panulirus guttatus
SO PEERJ
LA English
DT Article
DE Conservation; Population genetics; Neutral marker; Connectivity
ID POPULATION DIFFERENTIATION; GENETIC DIVERSITY; NULL ALLELES; ARGUS;
LOCI; SOFTWARE; PROGRAM; MARKERS
AB Microsatellite sequences were isolated from enriched genomic libraries of the spotted spiny lobster, Panulirus guttatus using 454 Pyro sequencing. Twenty-nine Previously developed polynaerase chain reaction primer pairs of Panulirus argus microsatellite loci were also tested for cross-sPecies amPlification in Pauulitus guttatus. In total, eight consistently amplifying, and polymorphic loci were characterized for 57 individuals collected in the Florida Keys and Bermuda. The number of alleles per locUs ranged from 8 to 20 and observed heterozygosities ranged from 0.409 to 0.958. Significant deviations from Hardy Weinberg equilibrium were found in one locus from Florida and three loci from Bermuda. Quality control testing indicated that all loci were easy to score, highly polymorphic and showed no evidence of linkage disequilibrium. Null alleles were detected in three loci with moderate frequencies ranging from (20% to 22 %). These eight microsatellites provide novel molecular markers for future conservation genetics research of P. guffaws.
C1 [Truelove, Nathan; Preziosi, Richard F.] Univ Manchester, Fac Life Sci, Manchester, Lancs, England.
[Behringer, Donald C.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA.
[Behringer, Donald C.] Univ Florida, Emerging Pathogens Inst, Gainesville, FL USA.
[Butler, Mark J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
[Truelove, Nathan] Smithsonian Museum Nat Hist, Smithsonian Marine Stn, Ft Pierce, FL USA.
RP Truelove, N (reprint author), Univ Manchester, Fac Life Sci, Manchester, Lancs, England.; Truelove, N (reprint author), Smithsonian Museum Nat Hist, Smithsonian Marine Stn, Ft Pierce, FL USA.
EM trueloven@si.edu
FU University of Manchester, Sustainable Consumption Institute; NSF
[OCE0929086]
FX NKT received funding from the University of Manchester, Sustainable
Consumption Institute. This work was funded in part by NSF grant
OCE0929086 to MJB and DCB. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 27
TC 0
Z9 0
U1 2
U2 11
PU PEERJ INC
PI LONDON
PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND
SN 2167-8359
J9 PEERJ
JI PeerJ
PD JAN 25
PY 2016
VL 4
AR e1467
DI 10.7717/peerj.1467
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC7MU
UT WOS:000369405200001
PM 26855853
ER
PT J
AU Pham, LM
DeVience, SJ
Casola, F
Lovchinsky, I
Sushkov, AO
Bersin, E
Lee, J
Urbach, E
Cappellaro, P
Park, H
Yacoby, A
Lukin, M
Walsworth, RL
AF Pham, Linh M.
DeVience, Stephen J.
Casola, Francesco
Lovchinsky, Igor
Sushkov, Alexander O.
Bersin, Eric
Lee, Junghyun
Urbach, Elana
Cappellaro, Paola
Park, Hongkun
Yacoby, Amir
Lukin, Mikhail
Walsworth, Ronald L.
TI NMR technique for determining the depth of shallow nitrogen-vacancy
centers in diamond
SO PHYSICAL REVIEW B
LA English
DT Article
ID NUCLEAR-MAGNETIC-RESONANCE; NANOSCALE RESOLUTION; ROOM-TEMPERATURE;
SPIN; SPECTROSCOPY; SENSITIVITY; SENSOR
AB We demonstrate a robust experimental method for determining the depth of individual shallow nitrogen-vacancy (NV) centers in diamond with similar to 1 nm uncertainty. We use a confocal microscope to observe single NV centers and detect the proton nuclear magnetic resonance (NMR) signal produced by objective immersion oil, which has well understood nuclear spin properties, on the diamond surface. We determine the NV center depth by analyzing the NV NMR data using a model that describes the interaction of a single NV center with the statistically polarized proton spin bath. We repeat this procedure for a large number of individual, shallow NV centers and compare the resulting NV depths to the mean value expected from simulations of the ion implantation process used to create the NV centers, with reasonable agreement.
C1 [Pham, Linh M.; Casola, Francesco; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[DeVience, Stephen J.; Sushkov, Alexander O.; Park, Hongkun] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
[Lovchinsky, Igor; Sushkov, Alexander O.; Bersin, Eric; Urbach, Elana; Park, Hongkun; Yacoby, Amir; Lukin, Mikhail; Walsworth, Ronald L.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
[Lee, Junghyun] MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Cappellaro, Paola] MIT, Dept Nucl Sci & Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Park, Hongkun; Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, 52 Oxford St, Cambridge, MA 02138 USA.
[Yacoby, Amir] Harvard Univ, Sch Engn & Appl Sci, 15 Oxford St, Cambridge, MA 02138 USA.
RP Walsworth, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Walsworth, RL (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.; Walsworth, RL (reprint author), Harvard Univ, Ctr Brain Sci, 52 Oxford St, Cambridge, MA 02138 USA.
EM rwalsworth@cfa.harvard.edu
RI DeVience, Stephen/D-7274-2012
OI DeVience, Stephen/0000-0003-3142-7296
FU DARPA (QuASAR program); MURI (QuISM program); NSF; Swiss National
Science Foundation (SNSF); Moore Foundation
FX This work was supported by DARPA (QuASAR program), MURI (QuISM program),
the NSF, the Swiss National Science Foundation (SNSF), and the Moore
Foundation. We gratefully acknowledge Fedor Jelezko for helpful
technical discussions.
NR 34
TC 5
Z9 5
U1 6
U2 32
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD JAN 25
PY 2016
VL 93
IS 4
AR 045425
DI 10.1103/PhysRevB.93.045425
PG 12
WC Physics, Condensed Matter
SC Physics
GA DC4XA
UT WOS:000369222400008
ER
PT J
AU Laux, P
Tralau, T
Tentschert, J
Blume, A
Al Dahouk, S
Baumler, W
Bernstein, E
Bocca, B
Alimonti, A
Colebrook, H
de Cuyper, C
Dahne, L
Hauri, U
Howard, PC
Janssen, P
Katz, L
Klitzman, B
Kluger, N
Krutak, L
Platzek, T
Scott-Lang, V
Serup, J
Teubner, W
Schreiver, I
Wilkniss, E
Luch, A
AF Laux, Peter
Tralau, Tewes
Tentschert, Jutta
Blume, Annegret
Al Dahouk, Sascha
Baeumler, Wolfgang
Bernstein, Eric
Bocca, Beatrice
Alimonti, Alessandro
Colebrook, Helen
de Cuyper, Christa
Daehne, Lars
Hauri, Urs
Howard, Paul C.
Janssen, Paul
Katz, Linda
Klitzman, Bruce
Kluger, Nicolas
Krutak, Lars
Platzek, Thomas
Scott-Lang, Victoria
Serup, Jorgen
Teubner, Wera
Schreiver, Ines
Wilkniss, Elena
Luch, Andreas
TI A medical-toxicological view of tattooing
SO LANCET
LA English
DT Review
ID RED TATTOO; SKIN INFECTIONS; PATCH-TEST; 1064 NM; LASER; INKS; PIGMENTS;
REMOVAL; BLACK; MICE
AB Long perceived as a form of exotic self-expression in some social fringe groups, tattoos have left their maverick image behind and become mainstream, particularly for young people. Historically, tattoo-related health and safety regulations have focused on rules of hygiene and prevention of infections. Meanwhile, the increasing popularity of tattooing has led to the development of many new colours, allowing tattoos to be more spectacular than ever before. However, little is known about the toxicological risks of the ingredients used. For risk assessment, safe intradermal application of these pigments needs data for toxicity and biokinetics and increased knowledge about the removal of tattoos. Other concerns are the potential for phototoxicity, substance migration, and the possible metabolic conversion of tattoo ink ingredients into toxic substances. Similar considerations apply to cleavage products that are formed during laser-assisted tattoo removal. In this Review, we summarise the issues of concern, putting them into context, and provide perspectives for the assessment of the acute and chronic health effects associated with tattooing.
C1 [Laux, Peter; Tralau, Tewes; Tentschert, Jutta; Blume, Annegret; Al Dahouk, Sascha; Platzek, Thomas; Schreiver, Ines; Wilkniss, Elena; Luch, Andreas] German Fed Inst Risk Assessment BfR, Dept Prod Safety, Berlin, Germany.
[Baeumler, Wolfgang] Univ Regensburg, Klin & Poliklin Dermatol, D-93053 Regensburg, Germany.
[Bernstein, Eric] Main Line Ctr Laser Surg, Ardmore, PA USA.
[Bocca, Beatrice; Alimonti, Alessandro] Ist Super Sanita, I-00161 Rome, Italy.
[Colebrook, Helen] Minist Hlth New Zealand, Wellington, New Zealand.
[de Cuyper, Christa] Acad Hosp St Jan, Brugge, Belgium.
[Daehne, Lars] Surflay Nanotec, Berlin, Germany.
[Hauri, Urs] Kantonales Lab Basel Stadt, Basel, Switzerland.
[Howard, Paul C.] US FDA, Natl Ctr Toxicol Res, Jefferson, AR 72079 USA.
[Janssen, Paul] Natl Inst Publ Hlth & Environm RIVM, Bilthoven, Netherlands.
[Katz, Linda] US FDA, College Pk, MD USA.
[Klitzman, Bruce] Duke Univ, Med Ctr, Durham, NC USA.
[Kluger, Nicolas] Univ Helsinki, Helsinki, Finland.
[Kluger, Nicolas] Helsinki Univ Hosp, Helsinki, Finland.
[Krutak, Lars] Smithsonian Inst, Washington, DC 20560 USA.
[Scott-Lang, Victoria] Royal Infirm Edinburgh NHS Trust, Edinburgh, Midlothian, Scotland.
[Serup, Jorgen] Bispebjerg Hosp, Dept Dermatol, Tattoo Clin, DK-2400 Copenhagen NV, Denmark.
[Teubner, Wera] BASF Schweiz AG, Basel, Switzerland.
RP Luch, A (reprint author), German Fed Inst Risk Assessment BfR, Dept Prod Safety, Berlin, Germany.
EM andreas.luch@bfr.bund.de
OI Al Dahouk, Sascha/0000-0003-3835-0818
FU BfR
FX The writing of this Review and the realisation of the 1st International
Conference on Tattoo Safety at the German Federal Institute for Risk
Assessment (BfR) in 2013 has been financially supported by intramural
grants of the BfR. This document does not reflect the official policy of
the USA Food and Drug Administration and the mention of specific
products does not constitute an endorsement.
NR 86
TC 10
Z9 10
U1 13
U2 28
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0140-6736
EI 1474-547X
J9 LANCET
JI Lancet
PD JAN 23
PY 2016
VL 387
IS 10016
BP 395
EP 402
DI 10.1016/S0140-6736(15)60215-X
PG 8
WC Medicine, General & Internal
SC General & Internal Medicine
GA DB4XI
UT WOS:000368516500038
PM 26211826
ER
PT J
AU Mistani, PA
Sales, LV
Pillepich, A
Sanchez-Janssen, R
Vogelsberger, M
Nelson, D
Rodriguez-Gomez, V
Torrey, P
Hernquist, L
AF Mistani, Pouria A.
Sales, Laura V.
Pillepich, Annalisa
Sanchez-Janssen, Ruben
Vogelsberger, Mark
Nelson, Dylan
Rodriguez-Gomez, Vicente
Torrey, Paul
Hernquist, Lars
TI On the assembly of dwarf galaxies in clusters and their efficient
formation of globular clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; galaxies: dwarf; galaxies: evolution; galaxies:
interactions; galaxies: star clusters: general
ID MOVING MESH COSMOLOGY; MASSIVE STAR-CLUSTERS; COLD DARK-MATTER;
VIRGO-CLUSTER; ELLIPTIC GALAXIES; ILLUSTRIS SIMULATION; STELLAR MASS;
LAMBDA-CDM; HIERARCHICAL COSMOLOGY; STRUCTURAL-PROPERTIES
AB Galaxy clusters contain a large population of low-mass dwarf elliptical galaxies whose exact origin is unclear: their colours, structural properties and kinematics differ substantially from those of dwarf irregulars in the field. We use the Illustris cosmological simulation to study differences in the assembly histories of dwarf galaxies (3 x 10(8) < M-*/M-circle dot < 10(10)) according to their environment. We find that cluster dwarfs achieve their maximum total and stellar mass on average similar to 8 and similar to 4.5 Gyr ago (or redshifts z = 1.0 and 0.4, respectively), around the time of infall into the clusters. In contrast, field dwarfs not subjected to environmental stripping reach their maximum mass at z = 0. These different assembly trajectories naturally produce a colour bimodality, with blue isolated dwarfs and redder cluster dwarfs exhibiting negligible star formation today. The cessation of star formation happens over median times 3.5-5 Gyr depending on stellar mass, and shows a large scatter (similar to 1-8 Gyr), with the lower values associated with starburst events that occur at infall through the virial radius or pericentric passages. We argue that such starbursts together with the early assembly of cluster dwarfs can provide a natural explanation for the higher specific frequency of globular clusters (GCs) in cluster dwarfs, as found observationally. We present a simple model for the formation and stripping of GCs that supports this interpretation. The origin of dwarf ellipticals in clusters is, therefore, consistent with an environmentally driven evolution of field dwarf irregulars. However, the z = 0 field analogues of cluster dwarf progenitors have today stellar masses a factor of similar to 3 larger - a difference arising from the early truncation of star formation in cluster dwarfs.
C1 [Mistani, Pouria A.; Sales, Laura V.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Sales, Laura V.; Pillepich, Annalisa; Nelson, Dylan; Rodriguez-Gomez, Vicente; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sanchez-Janssen, Ruben] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Vogelsberger, Mark; Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA.
RP Mistani, PA (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
EM pakba002@ucr.edu
OI Torrey, Paul/0000-0002-5653-0786; Rodriguez-Gomez,
Vicente/0000-0002-9495-0079
FU CURIE supercomputer at CEA/France as part of PRACE project [RA0844];
SuperMUC computer at the Leibniz Computing Centre, Germany [pr85je];
NASA [NNX12AC67G]; NSF [AST-1312095]; HST [HST-AR-13897]
FX We are grateful to Mario Abadi, James Bullock, Mike Cooper, Raja
Guhathakurtha, Julio Navarro, Diederik Kruijssen, Eric Peng, Elisa
Toloba and Carlos Vera-Ciro for insightful and stimulating discussions.
We would like to thank Shy Genel, Debora Sijacki and Volker Springel for
early access to the simulations and comments on the draft. Simulations
were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and
Stampede supercomputers at the Texas Advanced Computing Center as part
of XSEDE, the Kraken supercomputer at Oak Ridge National Laboratory as
part of XSEDE, the CURIE supercomputer at CEA/France as part of PRACE
project RA0844, and the SuperMUC computer at the Leibniz Computing
Centre, Germany, as part of project pr85je. LH acknowledges support from
NASA grant NNX12AC67G and NSF grant AST-1312095. AP acknowledges support
from the HST grant HST-AR-13897. We would like to thank the referee,
Hugo Martel, for a useful report that helped to improve the first
version.
NR 106
TC 8
Z9 8
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2016
VL 455
IS 3
BP 2323
EP 2336
DI 10.1093/mnras/stv2435
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TX
UT WOS:000368008200005
ER
PT J
AU Nelson, BE
Robertson, PM
Payne, MJ
Pritchard, SM
Deck, KM
Ford, EB
Wright, JT
Isaacson, HT
AF Nelson, Benjamin E.
Robertson, Paul M.
Payne, Matthew J.
Pritchard, Seth M.
Deck, Katherine M.
Ford, Eric B.
Wright, Jason T.
Isaacson, Howard T.
TI An empirically derived three-dimensional Laplace resonance in the Gliese
876 planetary system
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; methods: statistical; techniques: radial velocities;
planets and satellites: dynamical evolution and stability; planets and
satellites: formation
ID RADIAL-VELOCITY DATA; BAYESIAN MODEL SELECTION; MEAN MOTION RESONANCES;
EXOPLANET HOST STARS; N-BODY INTEGRATIONS; EXTRASOLAR PLANET; GIANT
PLANET; DYNAMICAL ANALYSIS; MIGRATING PLANETS; STELLAR ACTIVITY
AB We report constraints on the three-dimensional orbital architecture for all four planets known to orbit the nearby M dwarf Gliese 876 based solely on Doppler measurements and demanding long-term orbital stability. Our data set incorporates publicly available radial velocities taken with the ELODIE and CORALIE spectrographs, High Accuracy Radial velocity Planet Searcher (HARPS), and Keck HIgh Resolution Echelle Spectrometer (HIRES) as well as previously unpublished HIRES velocities. We first quantitatively assess the validity of the planets thought to orbit GJ 876 by computing the Bayes factors for a variety of different coplanar models using an importance sampling algorithm. We find that a four-planet model is preferred over a three-planet model. Next, we apply a Newtonian Markov chain Monte Carlo algorithm to perform a Bayesian analysis of the planet masses and orbits using an N-body model in three-dimensional space. Based on the radial velocities alone, we find that a 99 per cent credible interval provides upper limits on the mutual inclinations for the three resonant planets (Phi(cb) < 6.degrees 20 for the c and b pair and Phi(be) < 28.degrees 5 for the b and e pair). Subsequent dynamical integrations of our posterior sample find that the GJ 876 planets must be roughly coplanar (Phi(cb) < 2.degrees 60 and Phi(be) < 7.degrees 87), suggesting that the amount of planet-planet scattering in the system has been low. We investigate the distribution of the respective resonant arguments of each planet pair and find that at least one argument for each planet pair and the Laplace argument librate. The libration amplitudes in our three-dimensional orbital model support the idea of the outer three planets having undergone significant past disc migration.
C1 [Nelson, Benjamin E.; Robertson, Paul M.; Ford, Eric B.; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Nelson, Benjamin E.; Robertson, Paul M.; Ford, Eric B.; Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Payne, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pritchard, Seth M.] Univ Texas San Antonio, UTSA Circle, Dept Phys & Astron, San Antonio, TX 78249 USA.
[Deck, Katherine M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91101 USA.
[Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Nelson, BE (reprint author), Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA.
EM benelson@psu.edu
OI Nelson, Benjamin/0000-0003-3010-2334; Wright, Jason/0000-0001-6160-5888
FU NSF [AST-1126413]; Center for Exoplanets and Habitable Worlds; NASA
Origins of Solar Systems Program grant [NNX13A124G]; NASA Exoplanet
Science Institute [2007B N095Hr, 2010A N147Hr, 2011AB N141Hr, 2012A
N129Hr]; NASA Origins of Solar Systems grant [NNX09AB35G]; University of
Florida High Performance Computing Center; Pennsylvania State Research
Computing and Advanced Cyberinfrastructure Group; Pennsylvania State
University; Eberly College of Science; Pennsylvania Space Grant
Consortium
FX PR acknowledges support from NSF grant AST-1126413 and the Center for
Exoplanets and Habitable Worlds. MJP gratefully acknowledges the NASA
Origins of Solar Systems Program grant NNX13A124G. EBF and JTW
acknowledge NASA Keck PI Data Awards, administered by the NASA Exoplanet
Science Institute, including awards 2007B N095Hr, 2010A N147Hr, 2011A&B
N141Hr, and 2012A N129Hr. This research was supported by NASA Origins of
Solar Systems grant NNX09AB35G. We acknowledge the University of Florida
High Performance Computing Center and the Pennsylvania State Research
Computing and Advanced Cyberinfrastructure Group for providing
computational resources and support that have contributed to the results
reported within this paper. The Center for Exoplanets and Habitable
Worlds is supported by the Pennsylvania State University, the Eberly
College of Science, and the Pennsylvania Space Grant Consortium. We
extend special thanks to those of Hawaiian ancestry on whose sacred
mountain of Mauna Kea we are privileged to be guests. Without their
generous hospitality, the Keck observations presented herein would not
have been possible.
NR 98
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2016
VL 455
IS 3
BP 2484
EP 2499
DI 10.1093/mnras/stv2367
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TX
UT WOS:000368008200018
ER
PT J
AU Marshall, DW
Sadeghpour, HR
AF Marshall, David W.
Sadeghpour, H. R.
TI Simulating the formation of carbon-rich molecules on an idealized
graphitic surface
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE meteorites, meteors, meteoroids; dust, extinction; ISM: molecules
ID SIO LINE EMISSION; INTERSTELLAR JETS; SHOCK-WAVES; DYNAMICS;
HYDROCARBONS; GRAPHENE; OUTFLOWS; GRAINS; FILMS; WATER
AB There is accumulating evidence for the presence of complex molecules, including carbon-bearing and organic molecules, in the interstellar medium. Much of this evidence comes to us from studies of chemical composition, photo-and mass spectroscopy in cometary, meteoritic and asteroid samples, indicating a need to better understand the surface chemistry of astrophysical objects. There is also considerable interest in the origins of life-forming and life-sustaining molecules on the Earth. Here, we perform reactive molecular dynamics simulations to probe the formation of carbon-rich molecules and clusters on carbonaceous surfaces resembling dust grains and meteoroids. Our results show that large chains form on graphitic surfaces at low temperatures (100-500 K) and smaller fullerene-like molecules form at higher temperatures (2000-3000 K). The formation is faster on the surface than in the gas at low temperatures but slower at high temperatures as surface interactions prevent small clusters from coagulation. We find that for efficient formation of molecular complexity, mobility about the surface is important and helps to build larger carbon chains on the surface than in the gas phase at low temperatures. Finally, we show that the temperature of the surface strongly determines what kind of structures forms and that low turbulent environments are needed for efficient formation.
C1 [Marshall, David W.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Marshall, David W.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Marshall, DW (reprint author), Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
EM marshall@mps.mpg.de
FU University of Southampton Bursary Fund; NSF
FX DWM acknowledges the financial support from the University of
Southampton Bursary Fund and the NSF through a grant to the Institute
for Theoretical Atomic Molecular and Optical Physics. The authors thank
the anonymous referee for many valuable suggestions. While this
acknowledgment may be unusual, we feel that it is warranted, as the
referee should be credited for concise and precise comments on improving
the paper.
NR 44
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2016
VL 455
IS 3
BP 2889
EP 2900
DI 10.1093/mnras/stv2524
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TX
UT WOS:000368008200047
ER
PT J
AU Holoien, TWS
Kochanek, CS
Prieto, JL
Stanek, KZ
Dong, SB
Shappee, BJ
Grupe, D
Brown, JS
Basu, U
Beacom, JF
Bersier, D
Brimacombe, J
Danilet, AB
Falco, E
Guo, Z
Jose, J
Herczeg, GJ
Long, F
Pojmanski, G
Simonian, GV
Szczygiel, DM
Thompson, TA
Thorstensen, JR
Wagner, RM
Wozniak, PR
AF Holoien, T. W. -S.
Kochanek, C. S.
Prieto, J. L.
Stanek, K. Z.
Dong, Subo
Shappee, B. J.
Grupe, D.
Brown, J. S.
Basu, U.
Beacom, J. F.
Bersier, D.
Brimacombe, J.
Danilet, A. B.
Falco, E.
Guo, Z.
Jose, J.
Herczeg, G. J.
Long, F.
Pojmanski, G.
Simonian, G. V.
Szczygiel, D. M.
Thompson, T. A.
Thorstensen, J. R.
Wagner, R. M.
Wozniak, P. R.
TI Six months of multiwavelength follow-up of the tidal disruption
candidate ASASSN-14li and implied TDE rates from ASAS-SN
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: nuclei
ID MASSIVE BLACK-HOLE; DIGITAL SKY SURVEY; SWIFT ULTRAVIOLET/OPTICAL
TELESCOPE; ACTIVE GALACTIC NUCLEI; X-RAY TELESCOPE; DATA RELEASE;
GALAXY; STAR; SPECTROGRAPH; OUTBURST
AB We present ground-based and Swift photometric and spectroscopic observations of the candidate tidal disruption event (TDE) ASASSN-14li, found at the centre of PGC 043234 (d similar or equal to 90 Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source had a peak bolometric luminosity of L similar or equal to 10(44) erg s(-1) and a total integrated energy of E similar or equal to 7 x 10(50) erg radiated over the similar to 6 months of observations presented. The UV/optical emission of the source is well fitted by a blackbody with roughly constant temperature of T similar to 35 000 K, while the luminosity declines by roughly a factor of 16 over this time. The optical/UV luminosity decline is broadly consistent with an exponential decline, L proportional to e(-t/t0), with t(0) similar or equal to 60 d. ASASSN-14li also exhibits soft X-ray emission comparable in luminosity to the optical and UV emission but declining at a slower rate, and the X-ray emission now dominates. Spectra of the source show broad Balmer and helium lines in emission as well as strong blue continuum emission at all epochs. We use the discoveries of ASASSN-14li and ASASSN-14ae to estimate the TDE rate implied by ASAS-SN, finding an average rate of r similar or equal to 4.1 x 10(-5) yr(-1) per galaxy with a 90 per cent confidence interval of (2.2-17.0) x 10(-5) yr(-1) per galaxy. ASAS-SN found roughly 1 TDE for every 70 Type Ia supernovae in 2014, a rate that is much higher than that of other surveys.
C1 [Holoien, T. W. -S.; Kochanek, C. S.; Stanek, K. Z.; Brown, J. S.; Basu, U.; Beacom, J. F.; Simonian, G. V.; Thompson, T. A.; Wagner, R. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Holoien, T. W. -S.; Kochanek, C. S.; Stanek, K. Z.; Beacom, J. F.; Thompson, T. A.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, Columbus, OH 43210 USA.
[Prieto, J. L.] Univ Diego Portales, Nucleo Astron Fac Ingn, Santiago, Chile.
[Prieto, J. L.] Millennium Inst Astrophys, Santiago, Chile.
[Dong, Subo; Guo, Z.; Jose, J.; Herczeg, G. J.; Long, F.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Shappee, B. J.] Carnegie Observ, Pasadena, CA 91101 USA.
[Grupe, D.] Morehead State Univ, Dept Earth & Space Sci, Morehead, KY 40351 USA.
[Basu, U.] Grove City High Sch, Grove City, OH 43123 USA.
[Beacom, J. F.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Brimacombe, J.] Coral Towers Observ, Cairns, Qld 4870, Australia.
[Danilet, A. B.; Falco, E.] Smithsonian Inst, Whipple Observ, Amado, AZ 85645 USA.
[Pojmanski, G.; Szczygiel, D. M.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Thorstensen, J. R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Wagner, R. M.] Univ Arizona, LBT Observ, Tucson, AZ 85721 USA.
[Wozniak, P. R.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Holoien, TWS (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
EM tholoien@astronomy.ohio-state.edu
OI Wozniak, Przemyslaw/0000-0002-9919-3310
FU NSF [AST-0908816, PHY-1404311]; Center for Cosmology and AstroParticle
Physics at the Ohio State University; Mt. Cuba Astronomical Foundation;
DOE Computational Science Graduate Fellowship [DE-FG02-97ER25308];
FONDECYT [1151445]; Ministry of Economy, Development, and Tourism's
Millennium Science Initiative [IC120009]; Strategic Priority Research
Program 'The Emergence of Cosmological Structures of the Chinese Academy
of Sciences [XDB09000000]; NASA through Hubble Fellowship - Space
Telescope Science Institute [HST-HF-51348.001]; NASA [NAS 5-26555];
Laboratory Directed Research and Development programme at LANL; Ministry
of Finance; Association of Universities for Research in Astronomy, Inc.,
under NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; UK
Science and Technology Facilities Council; Robert Martin Ayers Sciences
Fund; Alfred P. Sloan Foundation; National Science Foundation; US
Department of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University; National Aeronautics and
Space Administration; [NAS5-00136]
FX Development of ASAS-SN has been supported by NSF grant AST-0908816 and
the Center for Cosmology and AstroParticle Physics at the Ohio State
University. ASAS-SN is supported in part by Mt. Cuba Astronomical
Foundation.; TW-SH is supported by the DOE Computational Science
Graduate Fellowship, grant number DE-FG02-97ER25308. Support for JLP is
in part provided by FONDECYT through the grant 1151445 and by the
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative through grant IC120009, awarded to The Millennium Institute
of Astrophysics, MAS. SD is supported by the Strategic Priority Research
Program 'The Emergence of Cosmological Structures of the Chinese Academy
of Sciences (Grant no. XDB09000000)'. BJS is supported by NASA through
Hubble Fellowship grant HST-HF-51348.001 awarded by the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.
JFB is supported by NSF grant PHY-1404311. PRW is supported by the
Laboratory Directed Research and Development programme at LANL.; This
research has made use of the XRT Data Analysis Software (XRTDAS)
developed under the responsibility of the ASI Science Data Center
(ASDC), Italy. At Penn State the NASA Swift programme is supported
through contract NAS5-00136.; This research uses data obtained through
the Telescope Access Program (TAP), which has also been funded by the
aforementioned Strategic Priority Research Program and the Special Fund
for Astronomy from the Ministry of Finance.; Observations made with the
NASA Galaxy Evolution Explorer (GALEX) were used in the analyses
presented in this manuscript. Some of the data presented in this paper
were obtained from the Mikulski Archive for Space Telescopes (MAST).
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX13AC07G and by other grants and contracts.; The LT is operated on the
island of La Palma by Liverpool John Moores University in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias with financial support from the UK Science and Technology
Facilities Council.; This research was made possible through the use of
the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert
Martin Ayers Sciences Fund.; Funding for SDSS-III has been provided by
the Alfred P. Sloan Foundation, the Participating Institutions, the
National Science Foundation, and the US Department of Energy Office of
Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is
managed by the Astrophysical Research Consortium for the Participating
Institutions of the SDSS-III Collaboration including the University of
Arizona, the Brazilian Participation Group, Brookhaven National
Laboratory, Carnegie Mellon University, University of Florida, the
French Participation Group, the German Participation Group, Harvard
University, the Instituto de Astrofisica de Canarias, the Michigan
State/Notre Dame/JINA Participation Group, Johns Hopkins University,
Lawrence Berkeley National Laboratory, Max Planck Institute for
Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University.; This publication makes
use of data products from the 2MASS, which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation.; This publication makes use of data products from the WISE,
which is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration.
NR 79
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 21
PY 2016
VL 455
IS 3
BP 2918
EP 2935
DI 10.1093/mnras/stv2486
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TX
UT WOS:000368008200049
ER
PT J
AU Chakraborti, S
Ray, A
Smith, R
Margutti, R
Pooley, D
Bose, S
Sutaria, F
Chandra, P
Dwarkadas, VV
Ryder, S
Maeda, K
AF Chakraborti, Sayan
Ray, Alak
Smith, Randall
Margutti, Raffaella
Pooley, David
Bose, Subhash
Sutaria, Firoza
Chandra, Poonam
Dwarkadas, Vikram V.
Ryder, Stuart
Maeda, Keiichi
TI PROBING FINAL STAGES OF STELLAR EVOLUTION WITH X-RAY OBSERVATIONS OF SN
2013ej
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; shock waves; stars: mass-loss; supernovae:
individual (SN 2013ej); X-rays: general
ID SUPERNOVA-REMNANTS; MASS-LOSS; IIL SUPERNOVA; LIGHT CURVES; EMISSION;
STARS; PROGENITOR; SHOCKS; 2009IP; M74
AB Massive stars shape their surroundings with mass loss from winds during their lifetimes. Fast ejecta from supernovae (SNe), from these massive stars, shock this circumstellar medium. Emission generated by this interaction provides a window into the final stages of stellar evolution, by probing the history of mass loss from the progenitor. Here we use Chandra and Swift. X-ray observations of the type II-P/L SN 2013ej to probe the history of mass loss from its progenitor. We model the observed X-rays as emission from both heated circumstellar matter and SN ejecta. The circumstellar density profile probed by the SN shock reveals a history of steady mass loss during the final 400 years. The inferred mass loss rate of 3 '10-6M(circle dot) yr(-1). points back to a 14 M-circle dot progenitor. Soon after the explosion we find significant absorption of reverse shock emission by a cooling shell. The column depth of this shell observed in absorption provides an independent and consistent measurement of the circumstellar density seen in emission. We also determine the efficiency of cosmic ray acceleration from X-rays produced by Inverse Compton scattering of optical photons by relativistic electrons. Only about 1% of the thermal energy is used to accelerate electrons. Our X-ray observations and modeling provide stringent tests for models of massive stellar evolution and micro-physics of shocks.
C1 [Chakraborti, Sayan; Ray, Alak] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
[Smith, Randall] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Margutti, Raffaella] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[Pooley, David] Trinity Univ, Dept Phys & Astron, San Antonio, TX 78212 USA.
[Bose, Subhash] Aryabhatta Res Inst Observat Sci, Manora Peak, Nainital, India.
[Sutaria, Firoza] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Chandra, Poonam] Natl Ctr Radio Astrophys, Pune Univ Campus, Pune 411007, Maharashtra, India.
[Dwarkadas, Vikram V.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Ryder, Stuart] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Maeda, Keiichi] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Chakraborti, Sayan] Harvard Univ, 78 Mt Auburn St, Cambridge, MA 02138 USA.
[Ray, Alak] Tata Inst Fundamental Res, 1 Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
RP Chakraborti, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.; Chakraborti, S (reprint author), Harvard Univ, 78 Mt Auburn St, Cambridge, MA 02138 USA.
EM schakraborti@fas.harvard.edu
FU National Aeronautics and Space Administration through Chandra
[G04-15076X]; National Aeronautics Space Administration [NAS8-03060];
Fulbright-Nehru Fellowship at Institute for Theory and Computation
(ITC), Harvard University
FX We acknowledge the use of public data from the Swift. data archive. This
research has made use of data obtained using the Chandra X-ray
Observatory through an advance Target of Opportunity program and
software provided by the Chandra X-ray Center (CXC) in the application
packages CIAO and ChIPS. Support for this work was provided by the
National Aeronautics and Space Administration through Chandra Award
Number G04-15076X issued by the Chandra X-ray Observatory Center, which
is operated by the Smithsonian Astrophysical Observatory for and on
behalf of the National Aeronautics Space Administration under contract
NAS8-03060. We thank Naveen Yadav for MESA runs and the anonymous
referee for useful suggestions. A.R. thanks the Fulbright Foundation for
a Fulbright-Nehru Fellowship at Institute for Theory and Computation
(ITC), Harvard University, and the Director and staff of ITC for their
hospitality during his sabbatical leave from Tata Institute of
Fundamental Research. At Tata Institute this research is part of 12th
Five Year Plan Project 12P-0261.
NR 54
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 22
DI 10.3847/0004-637X/817/1/22
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400022
ER
PT J
AU Chary, R
AF Chary, R.
TI SPECTRAL VARIATIONS OF THE SKY: CONSTRAINTS ON ALTERNATE UNIVERSES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; diffuse radiation;
surveys
ID COSMOLOGICAL HYDROGEN RECOMBINATION; MICROWAVE BACKGROUND SPECTRUM;
EMISSION
AB The fine tuning of parameters required to reproduce our present day universe suggests that our universe may simply be a region within an eternally inflating super-region. Many other regions beyond our observable universe would exist with each such region governed by a different set of physical parameters. Collision between these regions, if they occur, should leave signatures of anisotropy in the cosmic microwave background (CMB) but have not been seen. We analyze the spectral properties of masked, foreground-cleaned maps between 100 and 545 GHz constructed from the Planck data set. Four distinct similar to 2 degrees-4 degrees regions associated with CMB cold spots show anomalously strong 143 GHz emission but no correspondingly strong emission at either 100 or 217 GHz. The signal to noise of this 143 GHz residual emission is at the. greater than or similar to 6 sigma level which reduces to 3.2-5.4 sigma after subtraction of remaining synchrotron/free-free foregrounds. We assess different mechanisms for this residual emission and conclude that although there is a 30% probability that noise fluctuations may cause foregrounds to fall within 3 sigma of the excess, there is less than a 0.5% probability that foregrounds can explain all the excess. A plausible explanation is that the collision of our universe with an alternate universe whose baryon to photon ratio is a factor of similar to 4500 larger than ours, could produce enhanced hydrogen Paschen-series emission at the epoch of recombination. Future spectral mapping and deeper observations at 100 and 217 GHz are needed to mitigate systematics arising from unknown Galactic foregrounds and to confirm this unusual hypothesis.
C1 [Chary, R.] CALTECH, Infrared Proc & Anal Ctr, MS314-6, Pasadena, CA 91125 USA.
[Chary, R.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
RP Chary, R (reprint author), CALTECH, Infrared Proc & Anal Ctr, MS314-6, Pasadena, CA 91125 USA.; Chary, R (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM rchary@caltech.edu
NR 26
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 33
DI 10.3847/0004-637X/817/1/33
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400033
ER
PT J
AU Kenyon, SJ
Bromley, BC
AF Kenyon, Scott J.
Bromley, Benjamin C.
TI VARIATIONS ON DEBRIS DISKS. III. COLLISIONAL CASCADES AND GIANT IMPACTS
IN THE TERRESTRIAL ZONES OF SOLAR-TYPE STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planets and satellites:
formation; protoplanetary disks; stars: formation; zodiacal dust
ID SUN-LIKE STARS; ICY PLANET FORMATION; INFRARED INTERFEROMETRIC SURVEY;
SPITZER-SPACE-TELESCOPE; BODY-COAGULATION CODE; KUIPER-BELT OBJECTS;
MAIN-SEQUENCE STARS; SIZE DISTRIBUTION; DUSTY DEBRIS; WARM DUST
AB We analyze two new sets of coagulation calculations for solid particles orbiting within the terrestrial zone of a solar-type star. In models of collisional cascades, numerical simulations demonstrate that the total mass, the mass in 1 mm and smaller particles, and the dust luminosity decline with time more rapidly than predicted by analytic models, alpha t(-n) with n approximate to 1.1-1.2 instead of 1. Size distributions derived from the numerical calculations follow analytic predictions at r less than or similar to 0.1 km but are shallower than predicted at larger sizes. In simulations of planet formation, the dust luminosity declines more slowly than in pure collisional cascades, with n approximate to 0.5-0.8 instead of 1.1-1.2. Throughout this decline, giant impacts produce large, observable spikes in dust luminosity that last similar to 0.01-0.1 Myr and recur every 1-10 Myr. If most solar-type stars have Earth mass planets with a less than or similar to 1-2 AU, observations of debris around 1-100 Myr stars allow interesting tests of theory. Current data preclude theories where terrestrial planets form out of 1000 km or larger planetesimals. Although the observed frequency of debris disks among greater than or similar to 30 Myr old stars agrees with our calculations, the observed frequency of warm debris among 5-20 Myr old stars is smaller than predicted.
C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Bromley, Benjamin C.] Univ Utah, Dept Phys, 201 JFB, Salt Lake City, UT 84112 USA.
RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.; Bromley, BC (reprint author), Univ Utah, Dept Phys, 201 JFB, Salt Lake City, UT 84112 USA.
EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU NASA Astrophysics Theory and Origins of Solar Systems programs
[NNX10AF35G]; NASA Outer Planets Program [NNX11AM37G]
FX We acknowledge a generous allotment of computer time on the NASA
"discover" cluster. Comments from M. Geller, G. Kennedy, J. Najita, and
an anonymous referee improved our presentation. Portions of this project
were supported by the NASA Astrophysics Theory and Origins of Solar
Systems programs through grant NNX10AF35G and the NASA Outer Planets
Program through grant NNX11AM37G.
NR 187
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 51
DI 10.3847/0004-637X/817/1/51
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400051
ER
PT J
AU Marchesi, S
Civano, F
Elvis, M
Salvato, M
Brusa, M
Comastri, A
Gilli, R
Hasinger, G
Lanzuisi, G
Miyaji, T
Treister, E
Urry, CM
Vignali, C
Zamorani, G
Allevato, V
Cappelluti, N
Cardamone, C
Finoguenov, A
Griffiths, RE
Karim, A
Laigle, C
LaMassa, SM
Jahnke, K
Ranalli, P
Schawinski, K
Schinnerer, E
Silverman, JD
Smolcic, V
Suh, H
Trakhtenbrot, B
AF Marchesi, S.
Civano, F.
Elvis, M.
Salvato, M.
Brusa, M.
Comastri, A.
Gilli, R.
Hasinger, G.
Lanzuisi, G.
Miyaji, T.
Treister, E.
Urry, C. M.
Vignali, C.
Zamorani, G.
Allevato, V.
Cappelluti, N.
Cardamone, C.
Finoguenov, A.
Griffiths, R. E.
Karim, A.
Laigle, C.
LaMassa, S. M.
Jahnke, K.
Ranalli, P.
Schawinski, K.
Schinnerer, E.
Silverman, J. D.
Smolcic, V.
Suh, H.
Trakhtenbrot, B.
TI THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; cosmology: observations; galaxies: active; galaxies:
evolution; surveys; X-rays: general
ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; SUPERMASSIVE BLACK-HOLES;
WIDE-FIELD SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES;
MEDIUM-SENSITIVITY SURVEY; EVOLUTION SURVEY COSMOS; COMPTON-THICK AGN;
ROSAT DEEP SURVEY
AB We present the catalog of optical and infrared counterparts of the Chandra. COSMOS-Legacy. Survey, a 4.6 Ms Chandra. program on the 2.2 deg(2) of the COSMOS field, combination of 56 new overlapping observations obtained in Cycle 14 with the previous C-COSMOS survey. In this Paper we report the i, K, and 3.6 mu m identifications of the 2273 X-ray point sources detected in the new Cycle 14 observations. We use the likelihood ratio technique to derive the association of optical/infrared (IR) counterparts for 97% of the X-ray sources. We also update the information for the 1743 sources detected in C-COSMOS, using new K and 3.6 mu 3m information not available when the C-COSMOS analysis was performed. The final catalog contains 4016 X-ray sources, 97% of which have an optical/IR counterpart and a photometric redshift, while; similar or equal to 54% of the sources have a spectroscopic redshift. The full catalog, including spectroscopic and photometric redshifts and optical and X-ray properties described here in detail, is available online. We study several X-ray to optical (X/O) properties: with our large statistics we put better constraints on the X/O flux ratio locus, finding a shift toward faint optical magnitudes in both soft and hard X-ray band. We confirm the existence of a correlation between X/O and the the 2-10 keV luminosity for Type 2 sources. We extend to low luminosities the analysis of the correlation between the fraction of obscured AGNs and the hard band luminosity, finding a different behavior between the optically and X-ray classified obscured fraction.
C1 [Marchesi, S.; Civano, F.; Urry, C. M.; LaMassa, S. M.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA.
[Marchesi, S.; Civano, F.; Elvis, M.; Suh, H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Marchesi, S.; Brusa, M.; Lanzuisi, G.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Salvato, M.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Brusa, M.; Comastri, A.; Gilli, R.; Lanzuisi, G.; Vignali, C.; Zamorani, G.; Cappelluti, N.] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Hasinger, G.; Suh, H.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Km 103,Carret Tijunana Ensenada, Ensenada, Baja California, Mexico.
[Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile.
[Allevato, V.; Finoguenov, A.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, FI-00014 Helsinki, Finland.
[Cardamone, C.] Wheelock Coll, Dept Sci, Boston, MA 02215 USA.
[Griffiths, R. E.] Univ Hawaii, Div Nat Sci, Dept Phys & Astron, 200 W Kawili St, Hilo, HI 96720 USA.
[Karim, A.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
[Laigle, C.] Univ Paris 06, Sorbonne Univ, 98b Bd Arago, F-75014 Paris, France.
[Jahnke, K.] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
[Ranalli, P.] Lund Observ, POB 43, SE-22100 Lund, Sweden.
[Schawinski, K.; Trakhtenbrot, B.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Schinnerer, E.] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
[Schinnerer, E.] NRAO, 1003 Lopezville Rd, Socorro, NM 87801 USA.
[Silverman, J. D.] Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.
[Smolcic, V.] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, HR-10000 Zagreb, Croatia.
RP Marchesi, S (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA.; Marchesi, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Marchesi, S (reprint author), Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
RI Ranalli, Piero/K-6363-2013;
OI Ranalli, Piero/0000-0003-3956-755X; Cappelluti,
Nico/0000-0002-1697-186X; Schawinski, Kevin/0000-0001-5464-0888;
Zamorani, Giovanni/0000-0002-2318-301X; Trakhtenbrot,
Benny/0000-0002-3683-7297; Schinnerer, Eva/0000-0002-3933-7677; Urry,
Meg/0000-0002-0745-9792; Jahnke, Knud/0000-0003-3804-2137; Lanzuisi,
Giorgio/0000-0001-9094-0984
FU NASA Chandra grant [GO7-8136A]; PRIN-INAF; FP7 Career Integration Grant;
Collaborative Research Council 956; Deutsche Forschungsgemeinschaft
(DFG); UNAM-DGAPA [PAPIIT IN104113]; CONACyT Grant Cientifica Basica
[179662]; Greek General Secretariat of Research and Technology; NASA
[NNX15AE61G]; Swiss National Science Foundation [PP00P2_138979/1]; World
Premier International Research Center Initiative (WPI Initiative) MEXT,
Japan; Center of Excellence in Astrophysics and Associated Technologies
[PFB 06]; FONDECYT [1120061]; CONICYT [ACT1101]; European Union [337595,
333654]
FX This work was supported in part by NASA Chandra grant number GO7-8136A
(F.C., S.M., V.A., M.E.); PRIN-INAF 2014 "Windy Black Holes combing
galaxy evolution" (A.C., M.B., G.L. and C.V.); the FP7 Career
Integration Grant "eEASy": "Supermassive black holes through cosmic
time: from current surveys to eROSITA-Euclid Synergies" (CIG 321913;
M.B. and G.L.); the Collaborative Research Council 956, sub-project A1,
funded by the Deutsche Forschungsgemeinschaft (DFG; A.K.); UNAM-DGAPA
Grant PAPIIT IN104113 and CONACyT Grant Cientifica Basica #179662
(T.M.); the Greek General Secretariat of Research and Technology in the
framework of the programme Support of Postdoctoral Researchers (P.R.);
NASA award NNX15AE61G (R.G.); the Swiss National Science Foundation
Grant PP00P2_138979/1 (K.S.); the World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan (J.D.S.); the Center of
Excellence in Astrophysics and Associated Technologies (PFB 06), by the
FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101
(E.T.); the European Union's Seventh Framework programme under grant
agreements 337595 (ERC Starting Grant, "CoSMass") and 333654 (CIG, AGN
feedback; V.S.). B.T. is a Zwicky Fellow.
NR 128
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400034
ER
PT J
AU Martinez-Galarza, JR
Smith, HA
Lanz, L
Hayward, CC
Zezas, A
Rosenthal, L
Weiner, A
Hung, C
Ashby, MLN
Groves, B
AF Martinez-Galarza, J. R.
Smith, H. A.
Lanz, L.
Hayward, Christopher C.
Zezas, A.
Rosenthal, L.
Weiner, A.
Hung, C.
Ashby, M. L. N.
Groves, B.
TI VARIATIONS OF THE ISM COMPACTNESS ACROSS THE MAIN SEQUENCE OF STAR
FORMING GALAXIES: OBSERVATIONS AND SIMULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE evolution; galaxies: evolution; galaxies: interactions; galaxies:
starburst; galaxies: star formation
ID SPECTRAL ENERGY-DISTRIBUTION; SIMILAR-TO 2; SMOOTHED PARTICLE
HYDRODYNAMICS; ULTRALUMINOUS INFRARED GALAXIES; STARBURST GALAXIES;
MASSIVE GALAXIES; MOLECULAR GAS; COSMOLOGICAL SIMULATIONS; SUBMILLIMETER
GALAXIES; PHYSICAL-PROPERTIES
AB The majority of star-forming galaxies follow a simple empirical correlation in the star formation rate (SFR) versus stellar mass (M-*) plane, of the form SFR proportional to M-*(alpha), usually referred to as the star formation main sequence (MS). The physics that sets the properties of the MS is currently a subject of debate, and no consensus has been reached regarding the fundamental difference between members of the sequence and its outliers. Here we combine a set of hydro-dynamical simulations of interacting galactic disks with state-of-the-art radiative transfer codes to analyze how the evolution of mergers is reflected upon the properties of the MS. We present CHIBURST, a Markov Chain Monte Carlo spectral energy distribution (SED) code that fits the multi-wavelength, broad-band photometry of galaxies and derives stellar masses, SFRs, and geometrical properties of the dust distribution. We apply this tool to the SEDs of simulated mergers and compare the derived results with the reference output from the simulations. Our results indicate that changes in the SEDs of mergers as they approach coalescence and depart from the MS are related to an evolution of dust geometry in scales larger than a few hundred parsecs. This is reflected in a correlation between the specific star formation rate, and the compactness parameter., that parametrizes this geometry and hence the evolution of dust temperature (T-dust) with time. As mergers approach coalescence, they depart from the MS and increase their compactness, which implies that moderate outliers of the MS are consistent with late-type mergers. By further applying our method to real observations of luminous infrared galaxies (LIRGs), we show that the merger scenario is unable to explain these extreme outliers of the MS. Only by significantly increasing the gas fraction in the simulations are we able to reproduce the SEDs of LIRGs.
C1 [Martinez-Galarza, J. R.; Smith, H. A.; Hayward, Christopher C.; Zezas, A.; Weiner, A.; Hung, C.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Lanz, L.] CALTECH, Infrared Proc & Archival Ctr, MC 100-22, Pasadena, CA 91125 USA.
[Hayward, Christopher C.] CALTECH, TAPIR 350-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Zezas, A.] Univ Crete, Dept Phys, POB 2208, Iraklion 71003, Crete, Greece.
[Rosenthal, L.] Haverford Coll, 370 Lancaster Ave, Haverford, PA 19041 USA.
[Weiner, A.] RPI Inst, 110 8th St, Troy, NY 12180 USA.
[Hung, C.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Groves, B.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
RP Martinez-Galarza, JR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jmartine@cfa.harvard.edu
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Hayward,
Christopher/0000-0003-4073-3236
FU NASA [NNX10AD68G, NNX14AJ61G]; JPL RSA contracts [1369565, 1369566]; FAS
Research Computing Group at Harvard University
FX We thank the anonymous referee for very useful remarks on the paper. The
authors would also like to thank Dimitra Rigopoulou and Georgios Magdis
for providing the photometry for the z similar to 0.3 ULIRGs. J. R. M.
G., H. A. S. and L. L. acknowledge partial support from NASA grants
NNX10AD68G and NNX14AJ61G, and JPL RSA contracts 1369565 and 1369566.
This research has made use of NASAs Astrophysics Data System
Bibliographic Services. The simulations in this paper were performed on
the Odyssey cluster supported by the FAS Research Computing Group at
Harvard University.
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SN 0004-637X
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JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 76
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400076
ER
PT J
AU Mezcua, M
Civano, F
Fabbiano, G
Miyaji, T
Marchesi, S
AF Mezcua, M.
Civano, F.
Fabbiano, G.
Miyaji, T.
Marchesi, S.
TI A POPULATION OF INTERMEDIATE-MASS BLACK HOLES IN DWARF STARBURST
GALAXIES UP TO REDSHIFT=1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; Galaxies: dwarf; galaxies: starburst;
X-rays: galaxies
ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; DIGITAL
SKY SURVEY; SCALE RADIO-EMISSION; GLOBULAR-CLUSTER G1; Z QUASAR SURVEY;
STELLAR MASS; COSMOS SURVEY; HENIZE 2-10
AB We study a sample of similar to 50,000 dwarf starburst and late-type galaxies drawn from the COSMOS survey with the aim of investigating the presence of nuclear accreting black holes (BHs) as those seed BHs from which supermassive BHs could grow in the early universe. We divide the sample into five complete redshift bins up to z = 1.5 and perform an X-ray stacking analysis using the Chandra COSMOS-Legacy survey data. After removing the contribution from X-ray binaries and hot gas to the stacked X-ray emission, we still find an X-ray excess in the five redshift bins that can be explained by nuclear accreting BHs. This X-ray excess is more significant for z < 0.5. At higher redshifts, these active galactic nuclei could suffer mild obscuration, as indicated by the analysis of their hardness ratios. The average nuclear X-ray luminosities in the soft band are in the range 10(39)-10(40) erg s(-1). Assuming that the sources accrete at >= 1% the Eddington rate, their BH masses would be <= 10(5) M-circle dot, thus in the intermediate-mass BH regime, but their mass would be smaller than the one predicted by the BH-stellar mass relation. If instead the sources follow the correlation between BH mass and stellar mass, they would have sub-Eddington accreting rates of similar to 10(-3) and BH masses 1-9 x 10(5) M-circle dot. We thus conclude that a population of intermediate-mass BHs exists in dwarf starburst galaxies, at least up to z = 1.5, though their detection beyond the local universe is challenging due to their low luminosity and mild obscuration unless deep surveys are employed.
C1 [Mezcua, M.; Civano, F.; Fabbiano, G.; Marchesi, S.] Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
[Mezcua, M.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
[Civano, F.; Marchesi, S.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA.
[Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Km 103,Carret Tijuana Ensenada, Ensenada 22860, BC, Mexico.
[Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
RP Mezcua, M (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.; Mezcua, M (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
EM marmezcua.astro@gmail.com
FU NASA Chandra [G05-16099X, GO7-8136A]; UNAM-DGAPA Grant PAPIIT
[IN104113]; CONACyT Grant Cientifica Basica [179662]; Chandra Guest
Observer Support Grant [GO1-12178X]
FX We thank the referee Jenny Greene for her valuable comments which have
helped improve this manuscript. M.M. acknowledges financial support from
NASA Chandra Grant G05-16099X. This work was supported in part by NASA
Chandra grant number GO7-8136A (F.C. and S.M.). F.C. is gratefull to
Debra Fine for her support to women in science. T.M. acknowledges
support from UNAM-DGAPA Grant PAPIIT IN104113 and CONACyT Grant
Cientifica Basica #179662. The development of CSTACK was partially
supported by the Chandra Guest Observer Support Grant GO1-12178X.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
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SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400020
ER
PT J
AU Perley, DA
Kruhler, T
Schulze, S
Postigo, AD
Hjorth, J
Berger, E
Cenko, SB
Chary, R
Cucchiara, A
Ellis, R
Fong, W
Fynbo, JPU
Gorosabel, J
Greiner, J
Jakobsson, P
Kim, S
Laskar, T
Levan, AJ
Michalowski, MJ
Milvang-Jensen, B
Tanvir, NR
Thone, CC
Wiersema, K
AF Perley, D. A.
Kruhler, T.
Schulze, S.
de Ugarte Postigo, A.
Hjorth, J.
Berger, E.
Cenko, S. B.
Chary, R.
Cucchiara, A.
Ellis, R.
Fong, W.
Fynbo, J. P. U.
Gorosabel, J.
Greiner, J.
Jakobsson, P.
Kim, S.
Laskar, T.
Levan, A. J.
Michalowski, M. J.
Milvang-Jensen, B.
Tanvir, N. R.
Thoene, C. C.
Wiersema, K.
TI THE SWIFT GAMMA-RAY BURST HOST GALAXY LEGACY SURVEY. I. SAMPLE SELECTION
AND REDSHIFT DISTRIBUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: star formation;
gamma-ray burst: general; surveys
ID COSMIC STAR-FORMATION; CORE-COLLAPSE SUPERNOVAE; MASS-METALLICITY
RELATION; DARK GRB 080325; SIMILAR-TO 2; LUMINOSITY FUNCTION; OPTICAL
AFTERGLOW; FORMATION HISTORY; FORMING GALAXIES; ALERT TELESCOPE
AB We introduce the Swift Gamma-Ray Burst Host Galaxy Legacy Survey ("SHOALS"), a multi-observatory high-redshift galaxy survey targeting the largest unbiased sample of long-duration gamma-ray burst (GRB) hosts yet assembled (119 in total). We describe the motivations of the survey and the development of our selection criteria, including an assessment of the impact of various observability metrics on the success rate of afterglow-based redshift measurement. We briefly outline our host. galaxy observational program, consisting of deep Spitzer/IRAC imaging of every field supplemented by similarly deep, multicolor optical/near-IR photometry, plus spectroscopy of events without preexisting redshifts. Our optimized selection cuts combined with host. galaxy follow-up have so far enabled redshift measurements for 110 targets (92%) and placed upper limits on all but one of the remainder. About 20% of GRBs. in the sample are heavily dust. obscured, and at most 2% originate from z > 5.5. Using this sample, we estimate the redshift-dependent GRB rate density, showing it to peak at z similar to 2.5 and fall by at least an order of magnitude toward low (z = 0) redshift, while declining more gradually toward high (z similar to 7) redshift. This behavior is consistent with a progenitor whose formation efficiency varies modestly over cosmic history. Our survey will permit the most detailed examination to date of the connection between the GRB host population and general star-forming galaxies, directly measure evolution in the host population over cosmic time and discern its causes, and provide new constraints on the fraction of cosmic star formation occurring in undetectable galaxies at all redshifts.
C1 [Perley, D. A.; Ellis, R.] CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Perley, D. A.; Kruhler, T.; Hjorth, J.; Fynbo, J. P. U.; Milvang-Jensen, B.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Kruhler, T.] European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile.
[Schulze, S.; Kim, S.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Vicuna Mackenna 4860,7820436 Macul, Santiago 22, Chile.
[Schulze, S.; Kim, S.] Millennium Inst Astrophys, Vicuna Mackenna 4860,7820436 Macul, Santiago, Chile.
[de Ugarte Postigo, A.; Gorosabel, J.; Thoene, C. C.] CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain.
[Berger, E.; Laskar, T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Cenko, S. B.; Cucchiara, A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Chary, R.] US Planck Data Ctr, MS220-6, Pasadena, CA 91125 USA.
[Fong, W.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Greiner, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, Dunhagi 5, IS-107 Reykjavik, Iceland.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Michalowski, M. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Tanvir, N. R.; Wiersema, K.] Univ Leicester, Dept Phys & Ast3ron, Univ Rd, Leicester LE1 7RH, Leics, England.
RP Perley, DA (reprint author), CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA.; Perley, DA (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
EM dperley@dark-cosmology.dk
OI de Ugarte Postigo, Antonio/0000-0001-7717-5085; Kruehler,
Thomas/0000-0002-8682-2384; Thone, Christina/0000-0002-7978-7648;
Schulze, Steve/0000-0001-6797-1889
FU NASA [NAS 5-26555]; NASA - Space Telescope Science Institute
[HST-HF-51296.01-A]; Marie Sklodowska-Curie Individual Fellowship within
the Horizon 2020 European Union (EU) Framework Programme for Research
and Innovation [H2020-MSCA-IF-2014-660113]; DNRF; European Research
Council under the European Union's Seventh Framework Program (FP7)/ERC
Grant [EGGS-278202]; CONICYT-Chile FONDECYT [3140534]; Basal-CATA
[PFB-06/2007]; Millennium Institute of Astrophysics (MAS) of Iniciativa
Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
[IC120009]; FONDECYT [3130488]; NASA Postdoctoral Program at the Goddard
Space Flight Center; Ramon y Cajal fellowships; W. M. Keck Foundation;
Leibniz-Prize (DFG) [HA 1850/28-1]; [GO-90062]
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. It is
also based in part on observations with the NASA/ESA Hubble Space
Telescope, obtained from the Space Telescope Science Institute. STScI is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated
with program GO-90062. Support for this work was provided by NASA
through an award issued by JPL/Caltech. and through Hubble Fellowship
grant HST-HF-51296.01-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.
D.A.P. further acknowledges support from a Marie Sklodowska-Curie
Individual Fellowship within the Horizon 2020 European Union (EU)
Framework Programme for Research and Innovation
(H2020-MSCA-IF-2014-660113). The Dark Cosmology Centre is funded by the
DNRF. The research leading to these results has received funding from
the European Research Council under the European Union's Seventh
Framework Program (FP7/2007-2013)/ERC Grant agreement no. EGGS-278202.
S.S. acknowledges support from CONICYT-Chile FONDECYT 3140534,
Basal-CATA PFB-06/2007, and Project IC120009 "Millennium Institute of
Astrophysics (MAS) of Iniciativa Cientifica Milenio del Ministerio de
Economia, Fomento y Turismo. S.K. acknowledges support from FONDECYT
3130488. A.C. is supported by the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. A.d.U.P. and C.C.T. are
supported by Ramon y Cajal fellowships.; Some of the data presented here
were obtained at the W. M. Keck Observatory, which is operated as a
scientific partnership among the California Institute of Technology, the
University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. Based on observations made with ESO
Telescopes at the La Silla Paranal Observatory. and on observations made
with the Gran Telescopio Canarias (GTC). Part of the funding for GROND
(both hardware and personnel) was generously granted from the
Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).
NR 232
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 7
DI 10.3847/0004-637X/817/1/7
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400007
ER
PT J
AU Perley, DA
Tanvir, NR
Hjorth, J
Laskar, T
Berger, E
Chary, R
Postigo, AD
Fynbo, JPU
Kruhler, T
Levan, AJ
Michalowski, MJ
Schulze, S
AF Perley, D. A.
Tanvir, N. R.
Hjorth, J.
Laskar, T.
Berger, E.
Chary, R.
de Ugarte Postigo, A.
Fynbo, J. P. U.
Kruhler, T.
Levan, A. J.
Michalowski, M. J.
Schulze, S.
TI THE SWIFT GRB HOST GALAXY LEGACY SURVEY. II. REST-FRAME NEAR-IR
LUMINOSITY DISTRIBUTION AND EVIDENCE FOR A NEAR-SOLAR METALLICITY
THRESHOLD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: photometry;
galaxies: star formation; gamma-ray burst: general
ID GAMMA-RAY BURSTS; COSMIC STAR-FORMATION; CORE-COLLAPSE SUPERNOVAE;
SPITZER-SPACE-TELESCOPE; FORMATION RATE DENSITY; LYMAN BREAK GALAXIES;
SIMILAR-TO 2; HIGH-REDSHIFT; FORMING GALAXIES; MASSIVE STARS
AB We present rest-frame near-IR (NIR) luminosities and stellar masses for a large and uniformly selected population of gamma-ray burst (GRB) host galaxies using deep Spitzer Space Telescope imaging of 119 targets from the Swift GRB Host Galaxy Legacy Survey spanning 0.03 < z < 6.3, and we determine the effects of galaxy evolution and chemical enrichment on the mass distribution of the GRB host population across cosmic history. We find a rapid increase in the characteristic NIR host luminosity between z similar to 0.5 and z similar to 1.5, but little variation between z similar to 1.5 and z similar to 5. Dust-obscured GRBs dominate the massive host population but are only rarely seen associated with low-mass hosts, indicating that massive star-forming galaxies are universally and (to some extent) homogeneously dusty at high. redshift while low-mass star-forming galaxies retain little dust in their interstellar medium. Comparing our luminosity distributions with field surveys and measurements of the high-z mass-metallicity relation, our results have good consistency with a model in which the GRB rate per unit star formation is constant in galaxies with gas-phase metallicity below approximately the solar value but heavily suppressed in more metal-rich environments. This model also naturally explains the previously reported "excess" in the GRB rate beyond z greater than or similar to 2; metals stifle GRB production in most galaxies at z < 1.5 but have only minor impact at higher redshifts. The metallicity threshold we infer is much higher than predicted by single-star models and favors a binary progenitor. Our observations also constrain the fraction of cosmic star formation in low-mass galaxies undetectable to Spitzer to be small at z < 4.
C1 [Perley, D. A.] CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Perley, D. A.; Hjorth, J.; Fynbo, J. P. U.; Kruhler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
[Laskar, T.; Berger, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Chary, R.] US Planck Data Ctr, MS220-6, Pasadena, CA 91125 USA.
[de Ugarte Postigo, A.] CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain.
[Kruhler, T.] European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Michalowski, M. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Schulze, S.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Vicuna Mackenna 4860,7820436 Macul, Santiago 22, Chile.
[Schulze, S.] Millennium Inst Astrophys, Vicuna Mackenna 4860,7820436 Macul, Santiago, Chile.
RP Perley, DA (reprint author), CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA.; Perley, DA (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
EM dperley@dark-cosmology.dk
OI de Ugarte Postigo, Antonio/0000-0001-7717-5085; Kruehler,
Thomas/0000-0002-8682-2384; Schulze, Steve/0000-0001-6797-1889
FU NASA [GO-90062, NAS 5-26555]; NASA through Hubble Fellowship - Space
Telescope Science Institute [HST-HF-51296.01-A]; Marie Sklodowska-Curie
Individual Fellowship within the Horizon 2020 European Union (EU)
Framework Programme for Research and Innovation
[H2020-MSCA-IF-2014-660113]; DNRF; European Research Council under the
European Union's Seventh Framework Program (FP7)/ERC Grant
[EGGS-278202]; CONICYT-Chile FONDECYT [3140534]; Basal-CATA
[PFB-06/2007]; Millennium Institute of Astrophysics (MAS) of Iniciativa
Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
[IC120009]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech associated with program GO-90062.; Additional support for
this work was provided by NASA through Hubble Fellowship grant
HST-HF-51296.01-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555. D.A.P. further
acknowledges support from a Marie Sklodowska-Curie Individual Fellowship
within the Horizon 2020 European Union (EU) Framework Programme for
Research and Innovation (H2020-MSCA-IF-2014-660113).; The Dark Cosmology
Centre is funded by the DNRF. The research leading to these results has
received funding from the European Research Council under the European
Union's Seventh Framework Program (FP7/2007-2013)/ERC Grant agreement
no. EGGS-278202. S.S. acknowledges support from CONICYT-Chile FONDECYT
3140534, Basal-CATA PFB-06/2007, and Project IC120009 "Millennium
Institute of Astrophysics (MAS) of Iniciativa Cientifica Milenio del
Ministerio de Economia, Fomento y Turismo.
NR 98
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 8
DI 10.3847/0004-637X/817/1/8
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400008
ER
PT J
AU Sankrit, R
Raymond, JC
Blair, WP
Long, KS
Williams, BJ
Borkowski, KJ
Patnaude, DJ
Reynolds, SP
AF Sankrit, Ravi
Raymond, John C.
Blair, William P.
Long, Knox S.
Williams, Brian J.
Borkowski, Kazimierz J.
Patnaude, Daniel J.
Reynolds, Stephen P.
TI SECOND EPOCH HUBBLE SPACE TELESCOPE OBSERVATIONS OF KEPLER'S SUPERNOVA
REMNANT: THE PROPER MOTIONS OF BALMER FILAMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Kepler SN 1604, G4.5+6.8); ISM: supernova
remnants
ID SHOCK-WAVE; NONRADIATIVE SHOCKS; DOMINATED SHOCKS; ADVANCED CAMERA;
CYGNUS LOOP; SN 1006; EMISSION; NOVA; PROGENITOR; DUST
AB We report on the proper motions of Balmer-dominated filaments in Kepler's supernova remnant using high resolution images obtained with the Hubble Space Telescope at two epochs separated by about 10 years. We use the improved proper motion measurements and revised values of shock velocities to derive a distance to Kepler of 5.1(-70)(+0.8)kpc. The main shock around the northern rim of the remnant has a typical speed of 1690 km s(-1) and is encountering material with densities of about 8 cm(-3). We find evidence for the variation of shock properties over small spatial scales, including differences in the driving pressures as the shock wraps around a curved cloud surface. We find that the Balmer filaments ahead of the ejecta knot on the northwest boundary of the remnant are becoming fainter and more diffuse. We also find that the Balmer filaments associated with circumstellar material in the interior regions of the remnant are due to shocks with significantly lower velocities and that the brightness variations among these filaments trace the density distribution of the material, which may have a disk-like geometry.
C1 [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, M-S N211-3, Moffett Field, CA 94035 USA.
[Raymond, John C.; Patnaude, Daniel J.] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Blair, William P.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Long, Knox S.] Space Telescope Sci Inst, Cambridge, MA USA.
[Williams, Brian J.] NASA, GSFC, USRA, CRESST, Washington, DC USA.
[Williams, Brian J.] NASA, GSFC, Xray Astrophys Lab, Washington, DC USA.
[Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Raleigh, NC 27695 USA.
RP Sankrit, R (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr, M-S N211-3, Moffett Field, CA 94035 USA.
FU NASA [HST-GO-12885]
FX We thank Derek Hammer (previously of STScI) for his expertise with the
AstroDrizzle package and for providing us with the final aligned,
CTE-corrected images used for analysis. Figures 9 and 10 were made using
Veusz, a scientific plotting package written by Jeremy Sanders. This
work was supported in part by NASA grant HST-GO-12885, awarded to the
Universities Space Research Association and to the Johns Hopkins
University.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 36
DI 10.3847/0004-637X/817/1/36
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400036
ER
PT J
AU Savcheva, A
Pariat, E
McKillop, S
McCauley, P
Hanson, E
Su, Y
DeLuca, EE
AF Savcheva, A.
Pariat, E.
McKillop, S.
McCauley, P.
Hanson, E.
Su, Y.
DeLuca, E. E.
TI THE RELATION BETWEEN SOLAR ERUPTION TOPOLOGIES AND OBSERVED FLARE
FEATURES. II. DYNAMICAL EVOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun:
magnetic fields; Sun: X-rays, gamma rays
ID 3-DIMENSIONAL MAGNETIC RECONNECTION; SLIP-RUNNING RECONNECTION;
QUASI-SEPARATRIX LAYERS; POLAR CROWN PROMINENCE; X-RAY TELESCOPE; 2010
APRIL 8; ACTIVE-REGION; FLUX-ROPE; ELECTRIC-CURRENTS; 2-RIBBON FLARES
AB A long-established goal of solar physics is to build understanding of solar eruptions and develop flare and coronal mass ejection (CME) forecasting models. In this paper, we continue our investigation of nonlinear forces free field (NLFFF) models by comparing topological properties of the solutions to the evolution of the flare ribbons. In particular, we show that data-constrained NLFFF models of three erupting sigmoid regions (SOL2010-04-08, SOL2010-08-07, and SOL2012-05-12) built to reproduce the active region magnetic field in the pre-flare state can be rendered unstable and the subsequent sequence of unstable solutions produces quasi-separatrix layers that match the flare ribbon evolution as observed by SDO/AIA. We begin with a best-fit equilibrium model for the pre-flare active region. We then add axial flux to the flux rope in the model to move it across the stability boundary. At this point, the magnetofrictional code no longer converges to an equilibrium solution. The flux rope rises as the solutions are iterated. We interpret the sequence of magnetofrictional steps as an evolution of the active region as the flare/CME begins. The magnetic field solutions at different steps are compared with the flare ribbons. The results are fully consistent with the three-dimensional extension of the standard flare/CME model. Our ability to capture essential topological features of flaring active regions with a non-dynamic magnetofrictional code strongly suggests that the pre-flare, large-scale topological structures are preserved as the flux rope becomes unstable and lifts off.
C1 [Savcheva, A.; McKillop, S.; McCauley, P.; Su, Y.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Pariat, E.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris,PSL Res Univ, F-92190 Meudon, France.
[Hanson, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Su, Y.] Chinese Acad Sci, Key Lab Dark Matter & Space Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
RP Savcheva, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM asavcheva@cfa.harvard.edu
RI McCauley, Patrick/P-7747-2015;
OI McCauley, Patrick/0000-0002-1450-7350; DeLuca,
Edward/0000-0001-7416-2895
FU ESA, NSC (Norway); NASA [NNM07AB07C]; NASA LWS Jack Eddy postdoctoral
fellowship; NSFC [11333009]; Youth Fund of Jiang Su [BK20141043]; NAOJ
(UK); NASA (UK); STFC (UK)
FX Hinode is a Japanese mission developed, launched, and operated by
ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). Additional
operational support is provided by ESA, NSC (Norway). This work was
supported by NASA contract NNM07AB07C to SAO. The QSL computations have
been performed on the multi-processors TRU64 computer of the LESIA. A.S.
is supported by the NASA LWS Jack Eddy postdoctoral fellowship. Y.S. is
supported by NSFC # 11333009 and Youth Fund of Jiang Su # BK20141043. We
would like to thank the AIA team for supplying the data for this study.
NR 69
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2016
VL 817
IS 1
AR 43
DI 10.3847/0004-637X/817/1/43
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB9YA
UT WOS:000368872400043
ER
PT J
AU Archambault, S
Archer, A
Aune, T
Barnacka, A
Benbow, W
Bird, R
Buchovecky, M
Buckley, JH
Bugaev, V
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fleischhack, H
Flinders, A
Fortin, P
Fortson, L
Furniss, A
Gillanders, GH
Griffin, S
Grube, J
Gyuk, G
Hutten, M
Hakansson, N
Hanna, D
Holder, J
Humensky, TB
Johnson, CA
Kaaret, P
Kar, P
Kelley-Hoskins, N
Kertzman, M
Khassen, Y
Kieda, D
Krause, M
Krennrich, F
Kumar, S
Lang, MJ
Maier, G
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Mukherjee, R
Nieto, D
O'Brien, S
de Bhroithe, AO
Ong, RA
Otte, AN
Pandel, D
Park, N
Pelassa, V
Pohl, M
Popkow, A
Pueschel, E
Quinn, J
Ragan, K
Reynolds, PT
Richards, GT
Roache, E
Rousselle, J
Rulten, C
Santander, M
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Vincent, S
Wakely, SP
Weiner, OM
Weinstein, A
Wilhelm, A
Williams, DA
Zitzer, B
AF Archambault, S.
Archer, A.
Aune, T.
Barnacka, A.
Benbow, W.
Bird, R.
Buchovecky, M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Flinders, A.
Fortin, P.
Fortson, L.
Furniss, A.
Gillanders, G. H.
Griffin, S.
Grube, J.
Gyuk, G.
Huetten, M.
Hakansson, N.
Hanna, D.
Holder, J.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kelley-Hoskins, N.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krause, M.
Krennrich, F.
Kumar, S.
Lang, M. J.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Mukherjee, R.
Nieto, D.
O'Brien, S.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Pandel, D.
Park, N.
Pelassa, V.
Pohl, M.
Popkow, A.
Pueschel, E.
Quinn, J.
Ragan, K.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Rousselle, J.
Rulten, C.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Vincent, S.
Wakely, S. P.
Weiner, O. M.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
TI EXCEPTIONALLY BRIGHT TEV FLARES FROM THE BINARY LS I+61 degrees 303
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; gamma-rays: general; stars: individual (LS I+61
degrees 303, VER J0240+612); X-rays: binaries
ID GAMMA-RAY BINARIES; FERMI-LAT; EMISSION; LSI+61-DEGREES-303;
+61-DEGREES-303; PERIODICITY; PARAMETERS; SWIFT/XRT
AB The TeV binary system LS I +61 degrees 303 is known for its regular, non-thermal emission pattern that traces the orbital period of the compact object in its 26.5 day orbit around its B0 Ve star companion. The system typically presents elevated TeV emission around apastron passage with flux levels between 5% and 15% of the steady flux from the Crab Nebula (> 300 GeV). In this article, VERITAS observations of LS I + 61 degrees. 303 taken in late 2014 are presented, during which bright TeV flares around apastron at flux levels peaking above 30% of the Crab Nebula flux were detected. This is the brightest such activity from this source ever seen in the TeV regime. The strong outbursts have rise and fall times of less than a day. The short timescale of the flares, in conjunction with the observation of 10 TeV photons from LS I + 61 degrees 303 during the flares, provides constraints on the properties of the accelerator in the source.
C1 [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Aune, T.; Buchovecky, M.; Ong, R. A.; Popkow, A.; Rousselle, J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Benbow, W.; Cerruti, M.; Fortin, P.; Pelassa, V.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Collins-Hughes, E.; O'Brien, S.; Pueschel, E.; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Telezhinsky, I.; Vincent, S.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Rulten, C.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA.
[Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA.
[Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Smith, A. W.] Univ Maryland, NASA GSFC, College Pk, MD 20742 USA.
RP de Bhroithe, AO (reprint author), DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
EM anna.ofaolain.de.bhroithe@desy.de
RI Nieto, Daniel/J-7250-2015;
OI Nieto, Daniel/0000-0003-3343-0755; Bird, Ralph/0000-0002-4596-8563
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Helmholtz
Association; Fermi Cycle 7 Guest Investigator Program [NNH13ZDA001N]
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation and the
Smithsonian Institution, and by NSERC in Canada. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument. The VERITAS Collaboration
is grateful to Trevor Weekes for his seminal contributions and
leadership in the field of VHE gamma-ray astrophysics, which made this
study possible. A. O'FdB acknowledges support through the Young
Investigators Program of the Helmholtz Association. A. W. Smith
acknowledges support from the Fermi Cycle 7 Guest Investigator Program,
grant number NNH13ZDA001N.
NR 36
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2016
VL 817
IS 1
AR L7
DI 10.3847/2041-8205/817/1/L7
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AO
UT WOS:000369370900007
ER
PT J
AU van Dam, MA
McLeod, BA
Bouchez, AH
AF van Dam, Marcos A.
McLeod, Brian A.
Bouchez, Antonin H.
TI Dispersed fringe sensor for the Giant Magellan Telescope
SO APPLIED OPTICS
LA English
DT Article; Proceedings Paper
CT OSA Topical Meeting on Digital Holography and 3D Imaging (DH)
CY MAY, 2015
CL Shanghai, PEOPLES R CHINA
ID BAND PHASING ALGORITHM; FOURIER-TRANSFORM; MIRROR SEGMENTS; KECK
TELESCOPES
AB The Giant Magellan Telescope (GMT) consists of seven 8.365 m segments, with gaps of 0.345 m between adjacent segments. A unique challenge for GMT lies in phasing the segments and, in particular, how to measure segment piston optically while the telescope is in science operation. In this paper, we present a dispersed fringe sensor (DFS) to make these measurements using a novel algorithm. We show that using four off-axis DFSs operating at J-band with 10 ms exposures, we are able to measure segment piston to the required 50 nm accuracy every 30 s with over 90% sky coverage. (C) 2016 Optical Society of America
C1 [van Dam, Marcos A.] Flat Wavefronts, 21 Lascelles St, Christchurch 8022, New Zealand.
[McLeod, Brian A.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Bouchez, Antonin H.] Giant Magellan Telescope Observ Corp, POB 90933, Pasadena, CA 91109 USA.
RP van Dam, MA (reprint author), Flat Wavefronts, 21 Lascelles St, Christchurch 8022, New Zealand.
EM marcos@flatwavefronts.com
FU GMTO Corporation
FX GMTO Corporation.
NR 23
TC 4
Z9 4
U1 3
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 20
PY 2016
VL 55
IS 3
BP 539
EP 547
DI 10.1364/AO.55.000539
PG 9
WC Optics
SC Optics
GA DC2OD
UT WOS:000369055100042
PM 26835929
ER
PT J
AU Ade, PAR
Ahmed, Z
Aikin, RW
Alexander, KD
Barkats, D
Benton, SJ
Bischoff, CA
Bock, JJ
Bowens-Rubin, R
Brevik, JA
Buder, I
Bullock, E
Buza, V
Connors, J
Crill, BP
Duband, L
Dvorkin, C
Filippini, JP
Fliescher, S
Grayson, J
Halpern, M
Harrison, S
Hilton, GC
Hui, H
Irwin, KD
Karkare, KS
Karpel, E
Kaufman, JP
Keating, BG
Kefeli, S
Kernasovskiy, SA
Kovac, JM
Kuo, CL
Leitch, EM
Lueker, M
Megerian, KG
Netterfield, CB
Nguyen, HT
O'Brient, R
Ogburn, RW
Orlando, A
Pryke, C
Richter, S
Schwarz, R
Sheehy, CD
Staniszewski, ZK
Steinbach, B
Sudiwala, RV
Teply, GP
Thompson, KL
Tolan, JE
Tucker, C
Turner, AD
Vieregg, AG
Weber, AC
Wiebe, DV
Willmert, J
Wong, CL
Wu, WLK
Yoon, KW
AF Ade, P. A. R.
Ahmed, Z.
Aikin, R. W.
Alexander, K. D.
Barkats, D.
Benton, S. J.
Bischoff, C. A.
Bock, J. J.
Bowens-Rubin, R.
Brevik, J. A.
Buder, I.
Bullock, E.
Buza, V.
Connors, J.
Crill, B. P.
Duband, L.
Dvorkin, C.
Filippini, J. P.
Fliescher, S.
Grayson, J.
Halpern, M.
Harrison, S.
Hilton, G. C.
Hui, H.
Irwin, K. D.
Karkare, K. S.
Karpel, E.
Kaufman, J. P.
Keating, B. G.
Kefeli, S.
Kernasovskiy, S. A.
Kovac, J. M.
Kuo, C. L.
Leitch, E. M.
Lueker, M.
Megerian, K. G.
Netterfield, C. B.
Nguyen, H. T.
O'Brient, R.
Ogburn, R. W.
Orlando, A.
Pryke, C.
Richter, S.
Schwarz, R.
Sheehy, C. D.
Staniszewski, Z. K.
Steinbach, B.
Sudiwala, R. V.
Teply, G. P.
Thompson, K. L.
Tolan, J. E.
Tucker, C.
Turner, A. D.
Vieregg, A. G.
Weber, A. C.
Wiebe, D. V.
Willmert, J.
Wong, C. L.
Wu, W. L. K.
Yoon, K. W.
CA Keck Array Collaboration
BICEP2 Collaboration
TI Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck
Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID B-MODE POLARIZATION; SCALES; MAPS
AB We present results from an analysis of all data taken by the BICEP2 and Keck Array cosmic microwave background (CMB) polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK deg in Stokes Q and U in the 150 GHz band and 127 nK deg in the 95 GHz band. We take auto-and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 to 353 GHz. An excess over lensed Lambda CDM is detected at modest significance in the 95 x 150 BB spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23 x 95, or for correlation between the dust and synchrotron sky patterns in spectra such as 23 x 353. We take the likelihood of all the spectra for a multicomponent model including lensed Lambda CDM, dust, synchrotron, and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r) using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit r(0.05) < 0.09 at 95% confidence, which is robust to variations explored in analysis and priors. Combining these B-mode results with the (more model-dependent) constraints from Planck analysis of CMB temperature plus baryon acoustic oscillations and other data yields a combined limit r(0.05) < 0.07 at 95% confidence. These are the strongest constraints to date on inflationary gravitational waves.
C1 [Ade, P. A. R.; Sudiwala, R. V.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Ahmed, Z.; Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Thompson, K. L.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA.
[Ahmed, Z.; Grayson, J.; Irwin, K. D.; Karpel, E.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K. L.; Tolan, J. E.; Wu, W. L. K.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Hui, H.; Kefeli, S.; Lueker, M.; O'Brient, R.; Orlando, A.; Staniszewski, Z. K.; Steinbach, B.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Alexander, K. D.; Barkats, D.; Bischoff, C. A.; Bowens-Rubin, R.; Buder, I.; Buza, V.; Connors, J.; Harrison, S.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 42, Cambridge, MA 02138 USA.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Bock, J. J.; Crill, B. P.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Staniszewski, Z. K.; Turner, A. D.; Weber, A. C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bullock, E.; Pryke, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Buza, V.; Dvorkin, C.; Kovac, J. M.; Wong, C. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Duband, L.] CEA Grenoble, Serv Basses Temp, F-38054 Grenoble, France.
[Filippini, J. P.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.; Willmert, J.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Halpern, M.; Wiebe, D. V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hilton, G. C.; Irwin, K. D.] NIST, Boulder, CO 80305 USA.
[Kaufman, J. P.; Keating, B. G.; Orlando, A.; Teply, G. P.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Netterfield, C. B.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada.
[Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
RP Kovac, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 42, Cambridge, MA 02138 USA.; Pryke, C (reprint author), Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.; Kovac, JM (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.; Pryke, C (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM jmkovac@cfa.harvard.edu; pryke@physics.umn.edu
OI Barkats, Denis/0000-0002-8971-1954; Weber, Alfons/0000-0002-8222-6681
FU National Science Foundation [ANT-1145172, ANT-1145143, ANT-1145248];
Keck Foundation; JPL Research and Technology Development Fund; NASA
[06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at
Caltech; Canada Foundation for Innovation grant; U.S. DOE Office of
Science
FX The Keck Array project has been made possible through support from the
National Science Foundation under Grants No. ANT-1145172 (Harvard), No.
ANT-1145143 (Minnesota), and No. ANT-1145248 (Stanford), and from the
Keck Foundation (Caltech). The development of antenna-coupled detector
technology was supported by the JPL Research and Technology Development
Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA
APRA and SAT programs. The development and testing of focal planes were
supported by the Gordon and Betty Moore Foundation at Caltech. Readout
electronics were supported by a Canada Foundation for Innovation grant
to UBC. The computations in this Letter were run on the Odyssey cluster
supported by the FAS Science Division Research Computing Group at
Harvard University. The analysis effort at Stanford and SLAC is
partially supported by the U.S. DOE Office of Science. We thank the
staff of the U.S. Antarctic Program and, in particular, the South Pole
Station without whose help this research would not have been possible.
Most special thanks go to Robert Schwarz and Steffen Richter. We thank
all those who have contributed past efforts to the BICEP-Keck Array
series of experiments, including the BICEP1 team. We also thank the
Planck and WMAP teams for the use of their data.
NR 27
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U1 4
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JAN 20
PY 2016
VL 116
IS 3
AR 031302
DI 10.1103/PhysRevLett.116.031302
PG 9
WC Physics, Multidisciplinary
SC Physics
GA DB4ZX
UT WOS:000368523400001
PM 26849583
ER
PT J
AU Lidman, C
Ardila, F
Owers, M
Adami, C
Chiappetti, L
Civano, F
Elyiv, A
Finet, F
Fotopoulou, S
Goulding, A
Koulouridis, E
Melnyk, O
Menanteau, F
Pacaud, F
Pierre, M
Plionis, M
Surdej, J
Sadibekova, T
AF Lidman, C.
Ardila, F.
Owers, M.
Adami, C.
Chiappetti, L.
Civano, F.
Elyiv, A.
Finet, F.
Fotopoulou, S.
Goulding, A.
Koulouridis, E.
Melnyk, O.
Menanteau, F.
Pacaud, F.
Pierre, M.
Plionis, M.
Surdej, J.
Sadibekova, T.
TI The XXL Survey XIV. AAOmega Redshifts for the Southern XXL Field
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE catalogs; surveys; galaxies: clusters: general; galaxies: quasars:
general
ID DATA RELEASE; CATALOG; GALAXY
AB We present a catalogue containing the redshifts of 3 660 X-ray selected targets in the XXL southern field. The redshifts were obtained with the AAOmega spectrograph and 2dF fibre positioner on the Anglo-Australian Telescope. The catalogue contains 1 515 broad line AGN, 528 stars, and redshifts for 41 out of the 49 brightest X-ray selected clusters in the XXL southern field.
C1 [Lidman, C.; Ardila, F.; Owers, M.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Ardila, F.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Owers, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Adami, C.] Univ Aix Marseille, CNRS, Pole Etoile, LAM,OAMP, Site Chateau Gombert,38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Chiappetti, L.] IASF Milano, INAF, Via Bassini 15, I-20133 Milan, Italy.
[Civano, F.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06250 USA.
[Civano, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, 27 Akad Zabolotnoho St, UA-03680 Kiev, Ukraine.
[Elyiv, A.] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Finet, F.] Manora Peak, Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, Uttarakhand, India.
[Finet, F.; Surdej, J.] Univ Liege, Extragalact Astrophys & Space Observat AEOS, Allee 6 Aout,17 Sart Tilman,Bt B5c, B-4000 Liege, Belgium.
[Fotopoulou, S.; Goulding, A.] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland.
[Goulding, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Koulouridis, E.; Pierre, M.; Sadibekova, T.] CEA Saclay, Serv Astrophys AIM, F-91191 Gif Sur Yvette, France.
[Melnyk, O.] Taras Shevchenko Natl Univ Kyiv, Astron Observ, Observatorna Str 3, UA-04053 Kiev, Ukraine.
[Melnyk, O.] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, HR-10000 Zagreb, Croatia.
[Menanteau, F.] Univ Illinois, Dept Astron, W Green St, Urbana, IL 61801 USA.
[Menanteau, F.] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA.
[Pacaud, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Plionis, M.] Aristotle Univ Thessaloniki, Dept Phys, Thessaloniki, Greece.
RP Lidman, C (reprint author), Australian Astron Observ, N Ryde, NSW 2113, Australia.
EM clidman@aao.gov.au
RI Koulouridis, Elias/C-4731-2014;
OI Fotopoulou, Sotiria/0000-0002-9686-254X; Menanteau,
Felipe/0000-0002-1372-2534
FU Australian Astronomical Observatory [A/2013A/018, A/2013B/001];
NEWFELPRO fellowship project in Croatia; BMBF/DLR [50 OR 1117]; DFG [RE
1462-6]; DFG Transregio Programme [TR33]
FX Based in part on data acquired through the Australian Astronomical
Observatory, under programmes A/2013A/018 and A/2013B/001. O.M. is
grateful for the financial support provided by the NEWFELPRO fellowship
project in Croatia. F.P. acknowledges support from the BMBF/DLR grant 50
OR 1117, the DFG grant RE 1462-6 and the DFG Transregio Programme TR33.
NR 24
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U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1323-3580
EI 1448-6083
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PD JAN 19
PY 2016
VL 33
AR e001
DI 10.1017/pasa.2015.52
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB7OY
UT WOS:000368706400001
ER
PT J
AU Johannsen, T
Broderick, AE
Plewa, PM
Chatzopoulos, S
Doeleman, SS
Eisenhauer, F
Fish, VL
Genzel, R
Gerhard, O
Johnson, MD
AF Johannsen, Tim
Broderick, Avery E.
Plewa, Philipp M.
Chatzopoulos, Sotiris
Doeleman, Sheperd S.
Eisenhauer, Frank
Fish, Vincent L.
Genzel, Reinhard
Gerhard, Ortwin
Johnson, Michael D.
TI Testing General Relativity with the Shadow Size of Sgr A
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; HORIZON TELESCOPE
OBSERVATIONS; NO-HAIR THEOREM; GALACTIC-CENTER; STELLAR ORBITS;
ACCRETION; SIMULATIONS; MODELS; VLBI
AB In general relativity, the angular radius of the shadow of a black hole is primarily determined by its mass-to-distance ratio and depends only weakly on its spin and inclination. If general relativity is violated, however, the shadow size may also depend strongly on parametric deviations from the Kerr metric. Based on a reconstructed image of Sagittarius A* (Sgr A*) from a simulated one-day observing run of a seven-station Event Horizon Telescope (EHT) array, we employ a Markov chain Monte Carlo algorithm to demonstrate that such an observation can measure the angular radius of the shadow of Sgr A* with an uncertainty of similar to 1.5 mu as (6%). We show that existing mass and distance measurements can be improved significantly when combined with upcoming EHT measurements of the shadow size and that tight constraints on potential deviations from the Kerr metric can be obtained.
C1 [Johannsen, Tim; Broderick, Avery E.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Johannsen, Tim; Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Plewa, Philipp M.; Chatzopoulos, Sotiris; Eisenhauer, Frank; Genzel, Reinhard; Gerhard, Ortwin] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Doeleman, Sheperd S.; Fish, Vincent L.] MIT, Haystack Observ, Westford, MA 01886 USA.
[Doeleman, Sheperd S.; Johnson, Michael D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Genzel, Reinhard] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Genzel, Reinhard] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RP Johannsen, T (reprint author), Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.; Johannsen, T (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
FU Perimeter Institute for Theoretical Physics; Natural Sciences and
Engineering Research Council of Canada; Government of Canada through
Industry Canada; Province of Ontario through the Ministry of Research
and Innovation; National Science Foundation; Gordon and Betty Moore
Foundation [GBMF-3561]; Smithsonian Institution
FX T. J. is supported in part by Perimeter Institute for Theoretical
Physics. A. E. B. receives financial support from Perimeter Institute
for Theoretical Physics and the Natural Sciences and Engineering
Research Council of Canada through a Discovery Grant. Research at
Perimeter Institute is supported by the Government of Canada through
Industry Canada and by the Province of Ontario through the Ministry of
Research and Innovation. The Event Horizon Telescope is supported by
grants from the National Science Foundation, from the Gordon and Betty
Moore Foundation (Grant No. GBMF-3561), from the Smithsonian
Institution, and with generous equipment donations from Xilinx Inc. and
HGST Inc.
NR 60
TC 12
Z9 12
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JAN 19
PY 2016
VL 116
IS 3
AR 031101
DI 10.1103/PhysRevLett.116.031101
PG 5
WC Physics, Multidisciplinary
SC Physics
GA DB4ZV
UT WOS:000368523200001
PM 26849580
ER
PT J
AU Sues, HD
AF Sues, Hans-Dieter
TI Dating the origin of dinosaurs
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Editorial Material
ID CHANARES FORMATION; EARLY EVOLUTION; ARGENTINA
C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
EM suesh@si.edu
NR 17
TC 0
Z9 0
U1 3
U2 8
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 19
PY 2016
VL 113
IS 3
BP 480
EP 481
DI 10.1073/pnas.1523058113
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DB4BX
UT WOS:000368458800026
PM 26747603
ER
PT J
AU Garcia-Robledo, C
Kuprewicz, EK
Staines, CL
Erwin, TL
Kress, WJ
AF Garcia-Robledo, Carlos
Kuprewicz, Erin K.
Staines, Charles L.
Erwin, Terry L.
Kress, W. John
TI Limited tolerance by insects to high temperatures across tropical
elevational gradients and the implications of global warming for
extinction
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Cephaloleia; Chelobasis; CO1; CTmax; thermal limits
ID THERMAL LIMITS; CLIMATE-CHANGE; EVOLUTIONARY RESPONSES; LATITUDE;
PHYSIOLOGY; CONSERVATION; ECTOTHERMS; DROSOPHILA
AB The critical thermal maximum (CTmax), the temperature at which motor control is lost in animals, has the potential to determine if species will tolerate global warming. For insects, tolerance to high temperatures decreases with latitude, suggesting that similar patterns may exist along elevational gradients as well. This study explored how CTmax varies among species and populations of a group of diverse tropical insect herbivores, the rolled-leaf beetles, across both broad and narrow elevational gradients. Data from 6,948 field observations and 8,700 museum specimens were used to map the elevational distributions of rolled-leaf beetles on two mountains in Costa Rica. CTmax was determined for 1,252 individual beetles representing all populations across the gradients. Initial morphological identifications suggested a total of 26 species with populations at different elevations displaying contrasting upper thermal limits. However, compared with morphological identifications, DNA barcodes (cytochrome oxidase I) revealed significant cryptic species diversity. DNA barcodes identified 42 species and haplotypes across 11 species complexes. These 42 species displayed much narrower elevational distributions and values of CTmax than the 26 morphologically defined species. In general, species found at middle elevations and on mountaintops are less tolerant to high temperatures than species restricted to lowland habitats. Species with broad elevational distributions display high CTmax throughout their ranges. We found no significant phylogenetic signal in CTmax, geography, or elevational range. The narrow variance in CTmax values for most rolled-leaf beetles, especially high-elevation species, suggests that the risk of extinction of insects may be substantial under some projected rates of global warming.
C1 [Garcia-Robledo, Carlos; Kuprewicz, Erin K.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Garcia-Robledo, Carlos; Staines, Charles L.; Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
EM garciac@si.edu
FU Smithsonian Institution Postdoctoral Fellowship Program; Global Earth
Observatories Program; Office of the Under Secretary for Science;
National Geographic/Waitt Institute Grant [W149-11]; Smithsonian Small
Grants; Smithsonian Institution Barcode Network Funds; Smithsonian Pell
Grant
FX We thank D. J. Futuyma and two anonymous reviewers for their
constructive suggestions. We thank M. Kuzmina and C. Puente for
assistance with DNA barcode generation and analyses. This study was
supported by grants from the Smithsonian Institution Postdoctoral
Fellowship Program, the Global Earth Observatories Program, the Office
of the Under Secretary for Science, National Geographic/Waitt Institute
Grant W149-11 (to C.G.-R.), Smithsonian Small Grants, Smithsonian
Institution Barcode Network Funds, and the Smithsonian Pell Grant (to
W.J.K., T.L.E., and C.G.-R.).
NR 37
TC 9
Z9 10
U1 21
U2 76
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 19
PY 2016
VL 113
IS 3
BP 680
EP 685
DI 10.1073/pnas.1507681113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DB4BX
UT WOS:000368458800061
PM 26729867
ER
PT J
AU Levine, NM
Zhang, K
Longo, M
Baccini, A
Phillips, OL
Lewis, SL
Alvarez-Davila, E
de Andrade, ACS
Brienen, RJW
Erwin, TL
Feldpausch, TR
Mendoza, ALM
Vargas, PN
Prieton, A
Silva-Espejo, JE
Malhi, Y
Moorcroft, PR
AF Levine, Naomi M.
Zhang, Ke
Longo, Marcos
Baccini, Alessandro
Phillips, Oliver L.
Lewis, Simon L.
Alvarez-Davila, Esteban
Segalin de Andrade, Ana Cristina
Brienen, Roel J. W.
Erwin, Terry L.
Feldpausch, Ted R.
Monteagudo Mendoza, Abel Lorenzo
Nunez Vargas, Percy
Prieton, Adriana
Eduardo Silva-Espejo, Javier
Malhi, Yadvinder
Moorcroft, Paul R.
TI Ecosystem heterogeneity determines the ecological resilience of the
Amazon to climate change
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Amazon forests; biomass; ecological resilience; climate change;
ecosystem heterogeneity
ID RAIN-FOREST; TROPICAL FOREST; EXPERIMENTAL DROUGHT; VEGETATION DYNAMICS;
WOOD DENSITY; DRY-SEASON; CARBON; BIOMASS; SOILS; FUTURE
AB Amazon forests, which store similar to 50% of tropical forest carbon and play a vital role in global water, energy, and carbon cycling, are predicted to experience both longer and more intense dry seasons by the end of the 21st century. However, the climate sensitivity of this ecosystem remains uncertain: several studies have predicted large-scale die-back of the Amazon, whereas several more recent studies predict that the biome will remain largely intact. Combining remote-sensing and ground-based observations with a size-and age-structured terrestrial ecosystem model, we explore the sensitivity and ecological resilience of these forests to changes in climate. We demonstrate that water stress operating at the scale of individual plants, combined with spatial variation in soil texture, explains observed patterns of variation in ecosystem biomass, composition, and dynamics across the region, and strongly influences the ecosystem's resilience to changes in dry season length. Specifically, our analysis suggests that in contrast to existing predictions of either stability or catastrophic biomass loss, the Amazon forest's response to a drying regional climate is likely to be an immediate, graded, heterogeneous transition from high-biomass moist forests to transitional dry forests and woody savannah-like states. Fire, logging, and other anthropogenic disturbances may, however, exacerbate these climate change-induced ecosystem transitions.
C1 [Levine, Naomi M.; Zhang, Ke; Moorcroft, Paul R.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Levine, Naomi M.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
[Zhang, Ke] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73072 USA.
[Longo, Marcos] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Baccini, Alessandro] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[Phillips, Oliver L.; Lewis, Simon L.; Brienen, Roel J. W.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Lewis, Simon L.] UCL, Dept Geog, London WC1E 6BT, England.
[Alvarez-Davila, Esteban] Jardin Bot Medellin, Grp Invest Serv Ecosistem & Cambio Climat, Medellin 14, Colombia.
[Segalin de Andrade, Ana Cristina] Inst Nacl de Pesquisas da Amazonia, BR-69067375 Manaus, AM, Brazil.
[Erwin, Terry L.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA.
[Feldpausch, Ted R.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4SB, Devon, England.
[Monteagudo Mendoza, Abel Lorenzo] Jardin Bot Missouri, Oxapampa, Peru.
[Nunez Vargas, Percy; Eduardo Silva-Espejo, Javier] Univ Nacl San Antonio Abad Cusco, Cuzco, Peru.
[Prieton, Adriana] Inst Ciencias Nat, Bogota, Colombia.
[Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
RP Moorcroft, PR (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
EM paul_moorcroft@harvard.edu
RI Phillips, Oliver/A-1523-2011; Longo, Marcos/F-5033-2014; Feldpausch,
Ted/D-3436-2009; Zhang, Ke/B-3227-2012;
OI Phillips, Oliver/0000-0002-8993-6168; Longo, Marcos/0000-0001-5062-6245;
Feldpausch, Ted/0000-0002-6631-7962; Zhang, Ke/0000-0001-5288-9372;
Lewis, Simon/0000-0002-8066-6851; Levine, Naomi/0000-0002-4963-0535
FU Gordon and Betty Moore Foundation Andes-Amazon Initiative; National
Oceanic and Atmospheric Administration Climate and Global Change
fellowship; Natural Environment Research Council; Gordon and Betty Moore
Foundation; European Research Council; Royal Society-Wolfson Research
Merit Award
FX We thank Amazon Forest Inventory Network (RAINFOR) partners for
generously providing plot data, particularly T. Baker; G.
Lopez-Gonzalez; and the late S. Almeida, A. Gentry, and S. Patino.
Funding was provided by the Gordon and Betty Moore Foundation
Andes-Amazon Initiative and a National Oceanic and Atmospheric
Administration Climate and Global Change fellowship (to N.M.L.). RAINFOR
inventories have been funded by the Natural Environment Research Council
and the Gordon and Betty Moore Foundation. O.L.P. is supported by a
European Research Council Advanced Grant and is a Royal Society-Wolfson
Research Merit Award holder.
NR 49
TC 9
Z9 10
U1 29
U2 87
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 19
PY 2016
VL 113
IS 3
BP 793
EP 797
DI 10.1073/pnas.1511344112
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DB4BX
UT WOS:000368458800080
PM 26711984
ER
PT J
AU Angulo, A
Baldwin, CC
Robertson, DR
AF Angulo, Arturo
Baldwin, Carole C.
Robertson, D. Ross
TI A new species of Leptoderma Vaillant, 1886 (Osmeriformes:
Alepocephalidae) from the Pacific coast of Central America
SO ZOOTAXA
LA English
DT Article
DE Deep sea; eel-slickheads; El Salvador; tropical eastern Pacific Ocean
AB A new species of Leptoderma Vaillant, 1886 is described from a single specimen trawled at 1368-1406 m depth off El Salvador, Central America, tropical eastern Pacific. Leptoderma ospesca n. sp. can be readily distinguished from its congeners by the following combination of characters: dermal papillae absent along the lateral line, pectoral-fin rays 6, pelvicfin rays 5, pre-dorsal length 54.9% of SL, both dorsal and anal fins separated from the caudal fin, dorsal- and anal-fin rays long, procurrent caudal-fin rays numerous and extending far forward on caudal peduncle, caudal-fin rays 16, and total preural vertebrae 60. A key to the species of the genus is presented.
C1 [Angulo, Arturo] Univ Costa Rica, Museo Zool, 11501-2060 San Pedro de Montes de Oca, San Jose, Costa Rica.
[Angulo, Arturo] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, 11501-2060 San Pedro de Montes de Oca, San Jose, Costa Rica.
[Angulo, Arturo] Univ Estadual Paulista, Dept Zool & Bot, Lab Ictiol, Rua Cristovao Colombo 2265, BR-15054000 Sao Jose Do Rio Preto, SP, Brazil.
[Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Robertson, D. Ross] Smithsonian Trop Res Inst, Balboa, Panama.
RP Robertson, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
EM arturo.angs@gmail.com; baldwinc@si.edu; drr@stri.org
OI Angulo, Arturo/0000-0002-4587-1446
FU Smithsonian Institution Federal Barcode grant
FX Ross Robertson, who collected the specimen of L. ospesca during the
December 2010 survey along the Pacific coast of Central America by the
B/O Miguel Oliver, participated in that survey at the invitation of
Mario Gonzalez Recinos of OSPESCA. Acquisition of the B/O Miguel Oliver
Pacific fish specimens to the USNM collection was made possible by a
Smithsonian Institution Federal Barcode grant to Lee Weigt, Carole
Baldwin, and Amy Driskell in 2011. Accessioning of this material into
the USNM collection was facilitated by Diane Pitassy. Sandra Raredon
made the digital radiographs and photos of the preserved holotype.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 18
PY 2016
VL 4066
IS 4
BP 493
EP 500
PG 8
WC Zoology
SC Zoology
GA DC7CX
UT WOS:000369377500010
PM 27395850
ER
PT J
AU Valin, LC
Fiore, AM
Chance, K
Abad, GG
AF Valin, L. C.
Fiore, A. M.
Chance, K.
Abad, G. Gonzalez
TI The role of OH production in interpreting the variability of CH2O
columns in the southeast US
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE formaldehyde; hydroxyl; isoprene; methane
ID OZONE MONITORING INSTRUMENT; ISOPRENE EMISSIONS; FORMALDEHYDE COLUMNS;
ATMOSPHERIC OXIDATION; OMI OBSERVATIONS; MODEL; SPACE; PHOTOOXIDATION;
CHEMISTRY; SENSITIVITY
AB Formaldehyde (CH2O), a key atmospheric oxidation intermediate that is detectable from satellite-based UV/visible spectrometers, is primarily formed when hydroxyl radical (OH) reacts with volatile organic compounds (VOC) and is removed by photolysis, reaction with OH or deposition. We investigate the influence of OH and VOC variability on the CH2O column using a steady state model and the WRF-Chem regional chemical transport model over the southeast United States for the summer of 2012 (June-August). The steady state model indicates that the CH2O column primarily depends on OH production rates (P-OH) at low concentrations of OH (<3x10(6)moleculescm(-3)), on both P-OH and VOC reactivity (VOCR: sigma(i)k(i)[VOC](i)) at moderate concentrations of OH (3x10(6)-7x10(6)moleculescm(-3)) and on VOCR at high concentrations of OH (>7x10(6)moleculescm(-3)). When constrained with WRF-Chem values of boundary layer average P-OH and VOCR, the steady state model of CH2O explains most of the daily (r(2)=0.93) and average June-August (r(2)=0.97) spatial variance of the fully simulated cloud-free CH2O column. These findings imply that measurements of the CH2O column offer the potential to better understand the processes affecting oxidation, particularly in remote regions, where OH concentrations are low. The findings also suggest that the inference of VOC emissions based on measurements of CH2O, or any other intermediate oxidation species with a photolytic lifetime that is short relative to removal by reaction with OH (e.g., glyoxal), should carefully account for the influence of OH on the observed pattern, especially where OH concentrations are below 5x10(6)moleculescm(-3), as occurs in remote forests, where OH strongly varies, as occurs downwind of large nitrogen oxide (NOx: NO+NO2) emission sources, or where OH sources are potentially biased.
C1 [Valin, L. C.; Fiore, A. M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Fiore, A. M.] Columbia Univ, Dept Earth & Environm Studies, Palisades, NY USA.
[Chance, K.; Abad, G. Gonzalez] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Valin, LC (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
EM lcvalin@ldeo.columbia.edu
OI Gonzalez Abad, Gonzalo/0000-0002-8090-6480
FU NOAA Climate and Global Change Fellowship Program; NASA Air Quality
Applied Sciences Team [NNX12AF15G]
FX This work was supported by the NOAA Climate and Global Change Fellowship
Program (http://www.vsp.ucar.edu/cgc/) and by the NASA Air Quality
Applied Sciences Team (NNX12AF15G). We thank two anonymous reviewers and
Bryan Duncan for their thoughtful and helpful comments. We acknowledge
Eleanor Browne and Wendy Goliff for use of the RACM2 chemical mechanism
with updates to isoprene and monoterpene nitrate chemistry [Browne et
al., 2014]. We acknowledge the use of the WRF-Chem model Version 3.5.1
made available at
http://www2.mmm.ucar.edu/wrf/users/download/get_source.html. Model
results and tools used to generate production and loss rates in WRF-Chem
will be made available upon request to the corresponding author. We
acknowledge the use of OMI/Aura Formaldehyde (HCHO) Total Column 1-orbit
L2 Swath 13 x 24 km (V003) available at
http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/OMI/omhcho_v003.shtml.
We acknowledge the Atmospheric Chemistry Working Group of the WRF model
for providing the
ftp://aftp.fsl.noaa.gov/divisions/taq/emissions_data_2005/. We
acknowledge the use of MOZART-4 global model output and the use of the
WRF-Chem preprocessor tools (mozbc and bioemiss) both made available at
https://www2.acom.ucar.edu/wrf-chem/wrf-chem-tools-community provided by
the Atmospheric Chemistry Observations and Modeling Lab (ACOM) of NCAR.
NR 60
TC 4
Z9 4
U1 8
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 16
PY 2016
VL 121
IS 1
BP 478
EP 493
DI 10.1002/2015JD024012
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TH
UT WOS:000369845300029
ER
PT J
AU Shields, JK
Mader, HM
Caricchi, L
Tuffen, H
Mueller, S
Pistone, M
Baumgartner, L
AF Shields, J. K.
Mader, H. M.
Caricchi, L.
Tuffen, H.
Mueller, S.
Pistone, M.
Baumgartner, L.
TI Unravelling textural heterogeneity in obsidian: Shear-induced outgassing
in the Rocche Rosse flow
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Obsidian; Outgassing; Emplacement; Rocche Rosse; Heterogeneity
ID MAGNETIC-SUSCEPTIBILITY AMS; RHYOLITIC GLASSES; SILICIC VOLCANISM;
AEOLIAN ISLANDS; LAVA DOME; MAGMA FRAGMENTATION; WATER CONCENTRATION;
DISSOLVED WATER; CORDON-CAULLE; ERUPTIONS
AB Obsidian flow emplacement is a complex and understudied aspect of silicic volcanism. Of particular importance is the question of how highly viscous magma can lose sufficient gas in order to erupt effusively as a lava flow. Using an array of methods we study the extreme textural heterogeneity of the Rocche Rosse obsidian flow in Lipari, a 2 km long, 100 m thick, similar to 800 year old lava flow, with respect to outgassing and emplacement mechanisms. 2D and 3D vesicle analyses and density measurements are used to classify the lava into four textural types: 'glassy' obsidian (<15% vesicles), 'pumiceous' lava (>40% vesicles), high aspect ratio, 'shear banded' lava (20-40% vesicles) and low aspect ratio, 'frothy' obsidian with 30-60% vesicles. Textural heterogeneity is observed on all scales (m to mu m) and occurs as the result of strongly localised strain. Magnetic fabric, described by oblate and prolate susceptibility ellipsoids, records high and variable degrees of shearing throughout the flow. Total water contents are derived using both thermogravimetry and infrared spectroscopy to quantify primary (magmatic) and secondary (meteoric) water. Glass water contents are between 0.08-0.25 wt.%. Water analysis also reveals an increase in water content from glassy obsidian bands towards 'frothy' bands of 0.06-0.08 wt.%, reflecting preferential vesiculation of higher water bands and an extreme sensitivity of obsidian degassing to water content. We present an outgassing model that reconciles textural, volatile and magnetic data to indicate that obsidian is generated from multiple shear-induced outgassing cycles, whereby vesicular magma outgasses and densifies through bubble collapse and fracture healing to form obsidian, which then re-vesiculates to produce 'dry' vesicular magma. Repetition of this cycle throughout magma ascent results in the low water contents of the Rocche Rosse lavas and the final stage in the degassing cycle determines final lava porosity. Heterogeneities in lava rheology (vesicularity, water content, microlite content, viscosity) play a vital role in the structural evolution of an obsidian flow and overprint flow-scale morphology. Post-emplacement hydration also depends heavily on local strain, whereby connectivity of vesicles as a result of shear deformation governs sample rehydration by meteoric water, a process previously correlated to lava vesicularity alone. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Shields, J. K.; Mader, H. M.] Univ Bristol, Sch Earth Sci, Bristol, Avon, England.
[Caricchi, L.] Univ Geneva, Sect Earth & Environm Sci, Geneva, Switzerland.
[Tuffen, H.] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England.
[Mueller, S.] Johannes Gutenberg Univ Mainz, Inst Geosci, D-55122 Mainz, Germany.
[Pistone, M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Baumgartner, L.] Univ Lausanne, Inst Earth Sci, Lausanne, Switzerland.
RP Shields, JK (reprint author), Univ Bristol, Sch Earth Sci, Bristol, Avon, England.
EM jessie.shields@bristol.ac.uk
RI Tuffen, Hugh/A-5388-2009
FU NERC [NE/J500033/1]
FX This research was supported by NERC grant (NE/J500033/1). Additionally
the authors are grateful to the following: Charles Clapham and Donovan
Hawley for assistance with sample coring (Engineering Workshop,
University of Bristol), Richard Brooker for technical support during
FTIR sample preparation and analysis (Experimental Petrology Research
Laboratory, University of Bristol), and to Eva Hartung and David Floess
for performing magnetic susceptibility and anisotropy measurements
(Section of Earth and Environmental Sciences, University of Geneva). We
are grateful to Thomas Shea and an anonymous reviewer for their comments
which greatly improved the manuscript.
NR 115
TC 3
Z9 3
U1 8
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD JAN 15
PY 2016
VL 310
BP 137
EP 158
DI 10.1016/j.jvolgeores.2015.12.003
PG 22
WC Geosciences, Multidisciplinary
SC Geology
GA DF4ZT
UT WOS:000371362300013
ER
PT J
AU Iafolla, VA
Fiorenza, E
Lefevre, C
Lucchesi, DM
Lucente, M
Magnafico, C
Nozzoli, S
Peron, R
Santoli, F
Lorenzini, EC
Milyukov, V
Shapiro, II
Glashow, S
AF Iafolla, V. A.
Fiorenza, E.
Lefevre, C.
Lucchesi, D. M.
Lucente, M.
Magnafico, C.
Nozzoli, S.
Peron, R.
Santoli, F.
Lorenzini, E. C.
Milyukov, V.
Shapiro, I. I.
Glashow, S.
TI A proposal for a test of Weak Equivalence Principle with improved
accuracy using a cryogenic differential accelerometer installed on a
pendulum
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Weak Equivalence Principle; Differential accelerometer; GReAT; GReAT_G
ID GRAVITATIONAL MASS; GENERAL-RELATIVITY; EINSTEIN ELEVATOR
AB We present here the concept for a new experimental test of the Weak Equivalence Principle (WEP) carried out in the gravity field of the Sun. The WEP, stating the independence of the gravitational acceleration a body is subject to from its mass and composition, is at the basis of general relativity theory and more in general of metric theories of gravitation. It is therefore very important to test it to the precision allowable by current technology. The experiment here proposed aims at measuring the relative acceleration of two test masses in free fall, searching for a possible violation of the WEP, which would show up as a non-zero acceleration signal. The core of the experiment is constituted by a differential accelerometer with zero baseline, whose central elements are two test masses of different materials. This differential accelerometer is placed on a pendulum, in such a way as to make the common center of mass coincident with the center of mass of the pendulum itself. Ensuring a very precise centering, such a system should provide a high degree of attenuation of the local seismic noise, which together with an integration time of the order of tens of days would allow a test of the WEP with an accuracy improved by at least an order of magnitude with respect to the best measurements achieved so far. One of the strengths of this proposal is the know-how acquired from a previous study and technology development (GReAT: General Relativity Accuracy Test) that involved a test of the WEP in the gravity field of the Earth, in free fall inside a co-moving capsule released from a stratospheric balloon. The concept of the experiment is introduced, with particular attention to the differential accelerometer and its accommodation on the pendulum. A preliminary estimate of the attainable precision is given, along with a critical analysis of the associated challenges. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Iafolla, V. A.; Fiorenza, E.; Lefevre, C.; Lucchesi, D. M.; Lucente, M.; Magnafico, C.; Nozzoli, S.; Peron, R.; Santoli, F.] Ist Astrofis & Planetol Spaziali IAPS INAF, Via Fosso del Cavaliere, I-00133 Rome, Italy.
[Lorenzini, E. C.] Univ Padua, Dipartimento Ingn Ind, Via Venezia 1, Padua, Italy.
[Milyukov, V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skij Prospect 13, Moscow 119992, Russia.
[Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA USA.
[Glashow, S.] Boston Univ, Boston, MA 02215 USA.
RP Iafolla, VA (reprint author), Ist Astrofis & Planetol Spaziali IAPS INAF, Via Fosso del Cavaliere, I-00133 Rome, Italy.
EM valerio.iafolla@iaps.inaf.it
OI Lucente, Marco/0000-0002-5359-5437
NR 18
TC 1
Z9 1
U1 0
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JAN 15
PY 2016
VL 57
IS 2
BP 715
EP 723
DI 10.1016/j.asr.2015.11.013
PG 9
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DC4TR
UT WOS:000369213700016
ER
PT J
AU Gager, Y
Gimenez, O
O'Mara, MT
Dechmann, DKN
AF Gager, Yann
Gimenez, Olivier
Teague O'Mara, M.
Dechmann, Dina K. N.
TI Group size, survival and surprisingly short lifespan in socially
foraging bats
SO BMC ECOLOGY
LA English
DT Article
DE Cox proportional hazard model; Fitness; Molossus molossus; Multistate
mark-recapture model; Social foraging; Sociality
ID NORTH-AMERICAN BIRDS; BIG BROWN BATS; COLONY SIZE; LOCAL ENHANCEMENT;
MATING SYSTEMS; ECOLOGICAL DETERMINANTS; INBREEDING AVOIDANCE;
ECHOLOCATING BATS; EMBALLONURID BATS; EPTESICUS-FUSCUS
AB Background: The relationships between group size, survival, and longevity vary greatly among social species. Depending on demographic and ecological circumstances, there are both positive and negative effects of group size variation on individual survival and longevity. For socially foraging species in particular there may be an optimal group size that predicts maximum individual survival that is directly related to the potential for information transfer, social coordination, and costs of conspecific interference. Our aim was to investigate this central aspect of evolutionary ecology by focusing on a socially foraging bat, Molossus molossus. This species optimizes foraging success by eavesdropping on the echolocation calls of group members to locate ephemeral food patches. We expected to find the highest survival and longest lifespans in small groups as a consequence of a trade-off between benefits of information transfer on ephemeral resources and costs of conspecific interference.
Results: In a mark-recapture study of 14 mixed-sex M. molossus social groups in Gamboa, Panama, spanning several years we found the expected relatively small and intermediate, but stable groups, with a mean size of 9.6 +/- 6.7 adults and juveniles. We estimated survival proxies using Cox proportional hazard models and multistate-mark recapture models generated with recapture data as well as automated monitoring of roost entrances in a subset of the groups. Median survival of females was very short with 1.8 years and a maximum estimated longevity of 5.6 years. Contrary to our expectations, we found no relationship between variation in group size and survival, a result similar to few other studies.
Conclusions: Strong selection towards small group size may result from psychoacoustic and cognitive constraints related to acoustic interference in social foraging and the complexity of coordinated flight. The short lifespans were unexpected and may result from life at the energetic edge due to a highly specialized diet. The absence of a relationship between group size and survival may reflect a similar but optimized survival within the selected range of group sizes. We expect the pattern of small group sizes will be consistent in future research on species dependent on social information transfer about ephemeral resources.
C1 [Gager, Yann; Teague O'Mara, M.; Dechmann, Dina K. N.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany.
[Gager, Yann; Teague O'Mara, M.; Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, D-78464 Constance, Germany.
[Gager, Yann] Univ Konstanz, Int Max Planck Res Sch Organismal Biol, D-78464 Constance, Germany.
[Gimenez, Olivier] Univ Montpellier 3, Univ Montpellier, EPHE, CEFE UMR 5175,CNRS, F-34293 Montpellier 5, France.
[Teague O'Mara, M.] Univ Konstanz, Zukunftskolleg, D-78464 Constance, Germany.
[Teague O'Mara, M.; Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Gager, Y (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany.
EM yann.gager@gmail.com
RI Gimenez, Olivier/G-4281-2010;
OI O'Mara, M. Teague/0000-0002-6951-1648
FU German Research Foundation [DFG-GZ DE 1807/3-1]; International Max
Planck Research School for Organismal Biology
FX We thank Rachel Page and the members of the bat lab, as well as Julia
Cramer, Matthieu Menage, Marion Muturi, Sebastian Rikker and Sebastian
Stockmaier. We are grateful to the workshop of the University of
Konstanz for developing the automated transponder readers, especially
Georg Heine, Karl Hoerenberg, Harald Kautz and Harald Richter. We also
thank Martin Wikelski and Kamran Safi for scientific advice as well as
Brian Cusak, Marina Lehmann, Kim G. Mortega, Ireneusz Ruczynski,
Sebastian Stockmaier and two anonymous reviewers for valuable comments
on the manuscript. This work was funded by the German Research
Foundation (DFG-GZ DE 1807/3-1 to DKND) and the International Max Planck
Research School for Organismal Biology.
NR 99
TC 2
Z9 2
U1 5
U2 60
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1472-6785
J9 BMC ECOL
JI BMC Ecol.
PD JAN 15
PY 2016
VL 16
AR 2
DI 10.1186/s12898-016-0056-1
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA DB2FY
UT WOS:000368324900001
PM 26767616
ER
PT J
AU Dong, SB
Shappee, BJ
Prieto, JL
Jha, SW
Stanek, KZ
Holoien, TWS
Kochanek, CS
Thompson, TA
Morrell, N
Thompson, IB
Basu, U
Beacom, JF
Bersier, D
Brimacombe, J
Brown, JS
Bufano, F
Chen, P
Conseil, E
Danilet, AB
Falco, E
Grupe, D
Kiyota, S
Masi, G
Nicholls, B
Olivares, EF
Pignata, G
Pojmanski, G
Simonian, GV
Szczygiel, DM
Wozniak, PR
AF Dong, Subo
Shappee, B. J.
Prieto, J. L.
Jha, S. W.
Stanek, K. Z.
Holoien, T. W. -S.
Kochanek, C. S.
Thompson, T. A.
Morrell, N.
Thompson, I. B.
Basu, U.
Beacom, J. F.
Bersier, D.
Brimacombe, J.
Brown, J. S.
Bufano, F.
Chen, Ping
Conseil, E.
Danilet, A. B.
Falco, E.
Grupe, D.
Kiyota, S.
Masi, G.
Nicholls, B.
Olivares, F. E.
Pignata, G.
Pojmanski, G.
Simonian, G. V.
Szczygiel, D. M.
Wozniak, P. R.
TI ASASSN-15lh: A highly super-luminous supernova
SO SCIENCE
LA English
DT Article
ID GAMMA-RAY BURSTS; SUPERLUMINOUS SUPERNOVAE; IC SUPERNOVAE; LIGHT CURVES;
GALAXY; REDSHIFT; MAGNETAR
AB We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of M-u,M-AB = -23.5 +/- 0.1 and bolometric luminosity L-bol = (2.2 +/- 0.2) x 10(45) ergs s(-1), which is more than twice as luminous as any previously known supernova. It has several major features characteristic of the hydrogen-poor super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are currently poorly understood. In contrast to most previously known SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous galaxy (M-K approximate to -25.5) with little star formation. In the 4 months since first detection, ASASSN-15lh radiated (1.1 +/- 0.2) x 10(52) ergs, challenging the magnetar model for its engine.
C1 [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Shappee, B. J.; Thompson, I. B.] Carnegie Observ, Pasadena, CA 91101 USA.
[Prieto, J. L.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile.
[Prieto, J. L.; Olivares, F. E.; Pignata, G.] Millennium Inst Astrophys, Santiago, Chile.
[Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Stanek, K. Z.; Holoien, T. W. -S.; Kochanek, C. S.; Thompson, T. A.; Basu, U.; Beacom, J. F.; Brown, J. S.; Danilet, A. B.; Simonian, G. V.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Stanek, K. Z.; Holoien, T. W. -S.; Kochanek, C. S.; Thompson, T. A.; Beacom, J. F.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, Columbus, OH 43210 USA.
[Morrell, N.] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Beacom, J. F.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Brimacombe, J.] Coral Towers Observ, Cairns, Qld 4870, Australia.
[Bufano, F.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Chen, Ping] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Conseil, E.] Observ Strasbourg, AFOEV, F-67000 Strasbourg, France.
[Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Grupe, D.] Morehead State Univ, Dept Earth & Space Sci, Morehead, KY 40351 USA.
[Kiyota, S.] Variable Star Observers League Japan VSOLJ, Chiba 2730126, Japan.
[Masi, G.] Virtual Telescope Project, I-03023 Ceccano, Italy.
[Nicholls, B.] Mt Vernon Observ, Nelson, New Zealand.
[Olivares, F. E.; Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Pojmanski, G.; Szczygiel, D. M.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Wozniak, P. R.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Dong, SB (reprint author), Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China.
EM dongsubo@pku.edu.cn
OI Wozniak, Przemyslaw/0000-0002-9919-3310
FU CAS [XDB09000000]; NASA; FONDECYT [1151445, 3140326]; MAS project
[IC120009]; NSF CAREER award [AST-0847157]
FX We acknowledge B. Zhang, L. Ho, A. Gal-Yam, and B. Katz for comments;
NSF AST-1515927, OSU CCAPP, Mt. Cuba Astronomical Foundation, TAP, SAO,
CAS grant XDB09000000 (S.D.); NASA Hubble Fellowship (B.J.S.); FONDECYT
grant 1151445, MAS project IC120009 (J.L.P.); NSF CAREER award
AST-0847157 (S.W.J.); U.S. Department of Energy (DOE) DE-FG02-97ER25308
(T.W.-S.H.); NSF PHY-1404311 (J.F.B.); D. Victor for donating equipment
(BN); FONDECYT postdoctoral fellowship 3140326 (F.O.E.), and Los Alamos
National Laboratory Laboratory Directed Research and Development program
(P.R.W). B.J.S. is a Hubble and Carnegie-Princeton Fellow. All data used
in this paper are made public, including the photometric data (tables S1
to S6) and spectroscopic data at public repository WISeREP (26)
(http://wiserep.weizmann.ac.il).
NR 25
TC 22
Z9 22
U1 4
U2 14
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 15
PY 2016
VL 351
IS 6270
BP 257
EP 260
DI 10.1126/science.aac9613
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA9AM
UT WOS:000368098600036
PM 26816375
ER
PT J
AU Diaz, S
Kattge, J
Cornelissen, JHC
Wright, IJ
Lavorel, S
Dray, S
Reu, B
Kleyer, M
Wirth, C
Prentice, IC
Garnier, E
Bonisch, G
Westoby, M
Poorter, H
Reich, PB
Moles, AT
Dickie, J
Gillison, AN
Zanne, AE
Chave, J
Wright, SJ
Sheremet'ev, SN
Jactel, H
Baraloto, C
Cerabolini, B
Pierce, S
Shipley, B
Kirkup, D
Casanoves, F
Joswig, JS
Gunther, A
Falczuk, V
Ruger, N
Mahecha, MD
Gorne, LD
AF Diaz, Sandra
Kattge, Jens
Cornelissen, Johannes H. C.
Wright, Ian J.
Lavorel, Sandra
Dray, Stephane
Reu, Bjoern
Kleyer, Michael
Wirth, Christian
Prentice, I. Colin
Garnier, Eric
Boenisch, Gerhard
Westoby, Mark
Poorter, Hendrik
Reich, Peter B.
Moles, Angela T.
Dickie, John
Gillison, Andrew N.
Zanne, Amy E.
Chave, Jerome
Wright, S. Joseph
Sheremet'ev, Serge N.
Jactel, Herve
Baraloto, Christopher
Cerabolini, Bruno
Pierce, Simon
Shipley, Bill
Kirkup, Donald
Casanoves, Fernando
Joswig, Julia S.
Guenther, Angela
Falczuk, Valeria
Rueger, Nadja
Mahecha, Miguel D.
Gorne, Lucas D.
TI The global spectrum of plant form and function
SO NATURE
LA English
DT Article
ID LEAF ECONOMICS SPECTRUM; RELATIVE GROWTH-RATE; RAIN-FOREST TREES;
HAWAIIAN METROSIDEROS-POLYMORPHA; TRAIT-ENVIRONMENT RELATIONSHIPS;
KERNEL DENSITY-ESTIMATION; FOLIAR NITROGEN ISOTOPES; DRY-MATTER CONTENT;
SEED SIZE; PHOTOSYNTHETIC CAPACITY
AB Earth is home to a remarkable diversity of plant forms and life histories, yet comparatively few essential trait combinations have proved evolutionarily viable in today's terrestrial biosphere. By analysing worldwide variation in six major traits critical to growth, survival and reproduction within the largest sample of vascular plant species ever compiled, we found that occupancy of six-dimensional trait space is strongly concentrated, indicating coordination and trade-offs. Three-quarters of trait variation is captured in a two-dimensional global spectrum of plant form and function. One major dimension within this plane reflects the size of whole plants and their parts; the other represents the leaf economics spectrum, which balances leaf construction costs against growth potential. The global plant trait spectrum provides a backdrop for elucidating constraints on evolution, for functionally qualifying species and ecosystems, and for improving models that predict future vegetation based on continuous variation in plant form and function.
C1 [Diaz, Sandra; Falczuk, Valeria; Gorne, Lucas D.] Univ Nacl Cordoba, CONICET, Inst Multidisciplinario Biol Vegetal IMBIV, RA-5000 Cordoba, Argentina.
[Diaz, Sandra; Falczuk, Valeria; Gorne, Lucas D.] Univ Nacl Cordoba, FCEFyN, RA-5000 Cordoba, Argentina.
[Kattge, Jens; Wirth, Christian; Boenisch, Gerhard; Joswig, Julia S.; Guenther, Angela; Mahecha, Miguel D.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Kattge, Jens; Wirth, Christian; Rueger, Nadja; Mahecha, Miguel D.] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany.
[Cornelissen, Johannes H. C.] Vrije Univ, Dept Ecol Sci, Syst Ecol, NL-1081 HV Amsterdam, Netherlands.
[Wright, Ian J.; Prentice, I. Colin; Westoby, Mark] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia.
[Lavorel, Sandra] Univ Grenoble Alpes, CNRS, UMR 5553, Lab Ecol Alpine, F-38041 Grenoble 9, France.
[Dray, Stephane] Univ Lyon 1, CNRS, Lab Biometrie & Biol Evolut, UMR5558, F-69622 Villeurbanne, France.
[Reu, Bjoern] Univ Leipzig, Inst Biol, D-04103 Leipzig, Germany.
[Reu, Bjoern] Univ Ind Santander, Escuela Biol, Bucaramanga 680002, Colombia.
[Kleyer, Michael] Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, Landscape Ecol Grp, D-26111 Oldenburg, Germany.
[Wirth, Christian] Univ Leipzig, Dept Systemat Bot & Funct Biodivers, D-04103 Leipzig, Germany.
[Prentice, I. Colin] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, AXA Chair Biosphere & Climate Impacts, Grand Challenges Ecosyst, Ascot SL5 7PY, Berks, England.
[Prentice, I. Colin] Univ London Imperial Coll Sci Technol & Med, Environm & Grantham Inst, Climate Change & Environm, Ascot SL5 7PY, Berks, England.
[Garnier, Eric] Univ Montpellier 3, EPHE, CNRS, Ctr Ecol Fonct & Evolut,UMR 5175, F-34293 Montpellier 5, France.
[Poorter, Hendrik] Forschungszentrum Julich GmbH, Plant Sci IBG 2, D-52425 Julich, Germany.
[Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
[Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia.
[Moles, Angela T.] UNSW Australia, Sch Biol Earth & Environm Sci, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia.
[Dickie, John] Collections, Ardingly RH17 6TN, W Sussex, England.
[Gillison, Andrew N.] Ctr Biodivers Management, Yungaburra, Qld 4884, Australia.
[Zanne, Amy E.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.
[Zanne, Amy E.] Missouri Bot Garden, Ctr Conservat & Sustainable Dev, St Louis, MO 63121 USA.
[Chave, Jerome] CNRS, Lab Evolut & Divers Biol, UMR 5174, F-31062 Toulouse, France.
[Chave, Jerome] Univ Toulouse 3, F-31062 Toulouse, France.
[Wright, S. Joseph; Rueger, Nadja] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Sheremet'ev, Serge N.] Komarov Bot Inst, St Petersburg 197376, Russia.
[Jactel, Herve] INRA, UMR1202, BIOGECO, F-33610 Cestas, France.
[Jactel, Herve] Univ Bordeaux, BIOGECO, UMR 1202, F-33600 Pessac, France.
[Baraloto, Christopher] Florida Int Univ, Dept Biol Sci, Int Ctr Trop Bot, Miami, FL 33199 USA.
[Baraloto, Christopher] INRA, UMR Ecol Forets Guyane, Kourou 97310, French Guiana.
[Cerabolini, Bruno] Univ Insubria, Dept Theoret & Appl Sci, I-21100 Varese, Italy.
[Pierce, Simon] Univ Milan, Dept Agr & Environm Sci DiSAA, I-20133 Milan, Italy.
[Shipley, Bill] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada.
[Kirkup, Donald] Royal Bot Gardens Kew, Biodivers Informat & Spatial Anal, Richmond TW9 3AB, Surrey, England.
[Casanoves, Fernando] Ctr Agron Trop Invest & Ensenanza CATIE, Unidad Bioestadist, Turrialba 30501, Costa Rica.
RP Diaz, S (reprint author), Univ Nacl Cordoba, CONICET, Inst Multidisciplinario Biol Vegetal IMBIV, Casilla Correo 495, RA-5000 Cordoba, Argentina.
EM sandra.diaz@unc.edu.ar
RI iDiv, Deutsches Zentrum/B-5164-2016; Garnier, Eric/D-1650-2012; Ruger,
Nadja/J-6393-2015; Wright, Ian/G-4979-2012; Casanoves,
Fernando/I-3588-2016; Kattge, Jens/J-8283-2016; Moles,
Angela/C-3083-2008; Dray, Stephane/B-4107-2010; Poorter,
Hendrik/B-8062-2010; Wright, Stuart/M-3311-2013; Sheremetiev,
Serge/K-4891-2013
OI Pierce, Simon/0000-0003-1182-987X; Garnier, Eric/0000-0002-9392-5154;
Ruger, Nadja/0000-0003-2371-4172; Wright, Ian/0000-0001-8338-9143;
Casanoves, Fernando/0000-0001-8765-9382; Kattge,
Jens/0000-0002-1022-8469; Moles, Angela/0000-0003-2041-7762; Dray,
Stephane/0000-0003-0153-1105; Poorter, Hendrik/0000-0001-9900-2433;
Wright, Stuart/0000-0003-4260-5676; Sheremetiev,
Serge/0000-0002-0318-6766
FU TRY initiative on plant traits; DIVERSITAS/Future Earth; German Centre
for Integrative Biodiversity Research (iDiv) Halle-Jena-Leipzig; BACI
[ID 640176]; Universidad Nacional de Cordoba; CONICET; FONCyT [PICT
554]; SECyT (Argentina); Leverhulme Trust, UK; Inter-American Institute
for Global Change Research (IAI) [SGP-CRA2015]; US National Science
Foundation [GEO-1138881]
FX We are grateful to the many researchers who contributed to this study by
making their data available, helping to check information, and/or
providing comments at various stages. The study was supported by the TRY
initiative on plant traits (http://www.try-db.org). The TRY database is
hosted at the Max Planck Institute for Biogeochemistry (Jena, Germany)
and supported by DIVERSITAS/Future Earth, the German Centre for
Integrative Biodiversity Research (iDiv) Halle-Jena-Leipzig, and BACI
(grant ID 640176). The study has also been partially supported by the
following institutions and grants to S.Di.: Universidad Nacional de
Cordoba and CONICET, FONCyT (PICT 554) and SECyT (Argentina), The
Leverhulme Trust, UK, and Inter-American Institute for Global Change
Research (IAI) SGP-CRA2015 (supported by US National Science Foundation
grant GEO-1138881).
NR 263
TC 44
Z9 45
U1 114
U2 352
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 14
PY 2016
VL 529
IS 7585
BP 167
EP U73
DI 10.1038/nature16489
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA7WK
UT WOS:000368015700027
PM 26700811
ER
PT J
AU Kunstler, G
Falster, D
Coomes, DA
Hui, F
Kooyman, RM
Laughlin, DC
Poorter, L
Vanderwel, M
Vieilledent, G
Wright, SJ
Aiba, M
Baraloto, C
Caspersen, J
Cornelissen, JHC
Gourlet-Fleury, S
Hanewinkel, M
Herault, B
Kattge, J
Kurokawa, H
Onoda, Y
Penuelas, J
Poorter, H
Uriarte, M
Richardson, S
Ruiz-Benito, P
Sun, IF
Stahl, G
Swenson, NG
Thompson, J
Westerlund, B
Wirth, C
Zavala, MA
Zeng, HC
Zimmerman, JK
Zimmermann, NE
Westoby, M
AF Kunstler, Georges
Falster, Daniel
Coomes, David A.
Hui, Francis
Kooyman, Robert M.
Laughlin, Daniel C.
Poorter, Lourens
Vanderwel, Mark
Vieilledent, Ghislain
Wright, S. Joseph
Aiba, Masahiro
Baraloto, Christopher
Caspersen, John
Cornelissen, J. Hans C.
Gourlet-Fleury, Sylvie
Hanewinkel, Marc
Herault, Bruno
Kattge, Jens
Kurokawa, Hiroko
Onoda, Yusuke
Penuelas, Josep
Poorter, Hendrik
Uriarte, Maria
Richardson, Sarah
Ruiz-Benito, Paloma
Sun, I-Fang
Stahl, Goeran
Swenson, Nathan G.
Thompson, Jill
Westerlund, Bertil
Wirth, Christian
Zavala, Miguel A.
Zeng, Hongcheng
Zimmerman, Jess K.
Zimmermann, Niklaus E.
Westoby, Mark
TI Plant functional traits have globally consistent effects on competition
SO NATURE
LA English
DT Article
ID HAWAIIAN METROSIDEROS-POLYMORPHA; TROPICAL RAIN-FOREST; SUB-ARCTIC
FLORA; LEAF DRY MASS; WIDE-RANGE; LAND-USE; ECONOMICS SPECTRUM; ELEVATED
CO2; WOODY-PLANTS; QUERCUS-ILEX
AB Phenotypic traits and their associated trade-offs have been shown to have globally consistent effects on individual plant physiological functions(1-3), but how these effects scale up to influence competition, a key driver of community assembly in terrestrial vegetation, has remained unclear (4). Here we use growth data from more than 3 million trees in over 140,000 plots across the world to show how three key functional traits-wood density, specific leaf area and maximum height-consistently influence competitive interactions. Fast maximum growth of a species was correlated negatively with its wood density in all biomes, and positively with its specific leaf area in most biomes. Low wood density was also correlated with a low ability to tolerate competition and a low competitive effect on neighbours, while high specific leaf area was correlated with a low competitive effect. Thus, traits generate trade-offs between performance with competition versus performance without competition, a fundamental ingredient in the classical hypothesis that the coexistence of plant species is enabled via differentiation in their successional strategies(5). Competition within species was stronger than between species, but an increase in trait dissimilarity between species had little influence in weakening competition. No benefit of dissimilarity was detected for specific leaf area or wood density, and only a weak benefit for maximum height. Our trait-based approach to modelling competition makes generalization possible across the forest ecosystems of the world and their highly diverse species composition.
C1 [Kunstler, Georges] Irstea, UR EMGR, F-38402 St Martin Dheres, France.
[Kunstler, Georges] Univ Grenoble Alpes, F-38402 Grenoble, France.
[Kunstler, Georges; Falster, Daniel; Kooyman, Robert M.; Westoby, Mark] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia.
[Coomes, David A.] Univ Cambridge, Dept Plant Sci, Forest Ecol & Conservat Grp, Cambridge CB2 3EA, England.
[Hui, Francis] Australian Natl Univ, Inst Math Sci, Canberra, ACT 0200, Australia.
[Kooyman, Robert M.] Royal Bot Gardens & Domain Trust, Natl Herbarium New South Wales, Sydney, NSW 2000, Australia.
[Laughlin, Daniel C.] Univ Waikato, Environm Res Inst, Sch Sci, Hamilton 3240, New Zealand.
[Poorter, Lourens] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6708 PB Wageningen, Netherlands.
[Vanderwel, Mark] Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada.
[Vieilledent, Ghislain; Gourlet-Fleury, Sylvie] Cirad, UPR BSEF, F-34398 Montpellier, France.
[Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama.
[Aiba, Masahiro; Kurokawa, Hiroko] Tohoku Univ, Sch Life Sci, Sendai, Miyagi 9808578, Japan.
[Baraloto, Christopher] INRA, UMR Ecol Forets Guyane, F-97387 Kourou, France.
[Baraloto, Christopher] Florida Int Univ, Dept Biol Sci, Int Ctr Trop Bot, Miami, FL 33199 USA.
[Caspersen, John; Zeng, Hongcheng] Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada.
[Caspersen, John; Zimmermann, Niklaus E.] Swiss Fed Res Inst WSL, Landscape Dynam Unit, CH-8903 Birmensdorf, Switzerland.
[Cornelissen, J. Hans C.] Vrije Univ, Dept Ecol Sci, Syst Ecol, NL-1081 HV Amsterdam, Netherlands.
[Hanewinkel, Marc] Swiss Fed Res Inst WSL, Forest Resources & Management Unit, CH-8903 Birmensdorf, Switzerland.
[Hanewinkel, Marc] Univ Freiburg, Chair Forestry Econ & Planning, D-79106 Freiburg, Germany.
[Herault, Bruno] Cirad, UMR Ecol Forets Guyane, F-97387 Kourou, France.
[Kattge, Jens] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Kattge, Jens; Wirth, Christian] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany.
[Onoda, Yusuke] Kyoto Univ, Sch Agr, Kyoto 6068502, Japan.
[Penuelas, Josep] UAB, CSIC, CREAF, Global Ecol Unit, Catalonia 08193, Spain.
[Penuelas, Josep] CREAF, Barcelona 08193, Catalonia, Spain.
[Poorter, Hendrik] Forschungszentrum Julich GmbH, Plant Sci IBG 2, D-52425 Julich, Germany.
[Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Richardson, Sarah] Landcare Res, Lincoln 7640, New Zealand.
[Ruiz-Benito, Paloma] Univ Stirling, Sch Nat Sci, Biol & Environm Sci, Stirling FK9 4LA, Scotland.
[Ruiz-Benito, Paloma; Zavala, Miguel A.] Univ Alcala De Henares, Dept Life Sci, Forest Ecol & Restorat Grp, Alcala De Henares 28805, Madrid, Spain.
[Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan.
[Stahl, Goeran; Westerlund, Bertil] Swedish Univ Agr Sci SLU, Dept Forest Resource Management, S-90183 Umea, Sweden.
[Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Thompson, Jill] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland.
[Thompson, Jill; Zimmerman, Jess K.] Univ Puerto Rico, Dept Environm Sci, San Juan, PR 00936 USA.
[Wirth, Christian] Univ Leipzig, Inst Systemat Bot & Funct Biodivers, D-04103 Leipzig, Germany.
RP Kunstler, G (reprint author), Irstea, UR EMGR, 2 Rue Papeterie BP 76, F-38402 St Martin Dheres, France.
EM georges.kunstler@irstea.fr
RI Zavala, Miguel/H-3603-2015; Poorter, Hendrik/B-8062-2010; Wright,
Stuart/M-3311-2013; Thompson, Jill/K-2200-2012; iDiv, Deutsches
Zentrum/B-5164-2016; Zimmermann, Niklaus/A-4276-2008; Hanewinkel,
Marc/E-5639-2011; Kattge, Jens/J-8283-2016; Kunstler,
Georges/F-9179-2012; Vieilledent, Ghislain/D-8323-2011
OI Penuelas, Josep/0000-0002-7215-0150; Ruiz-Benito,
Paloma/0000-0002-2781-5870; Herault, Bruno/0000-0002-6950-7286; Falster,
Daniel/0000-0002-9814-092X; Zavala, Miguel/0000-0003-1456-0132; Poorter,
Hendrik/0000-0001-9900-2433; Wright, Stuart/0000-0003-4260-5676;
Thompson, Jill/0000-0002-4370-2593; Zimmermann,
Niklaus/0000-0003-3099-9604; Hanewinkel, Marc/0000-0003-4081-6621;
Kattge, Jens/0000-0002-1022-8469; Kunstler, Georges/0000-0002-2544-1940;
Vieilledent, Ghislain/0000-0002-1685-4997
FU CEBA [ANR-10-LABX-25-01]; IGBP; DIVERSITAS; GLP; NERC; QUEST; FRB; GIS
Climate; Marie Curie International Outgoing Fellowship within European
Community [299340]; Macquarie University; Australian Research Council
FX We are especially grateful to the researchers whose long-term commitment
to establish and maintain forest plots and their associated databases
made this study possible, and to those who granted us data access:
forest inventories and permanent plots of New Zealand, Spain (MAGRAMA),
France, Switzerland, Sweden, US and Canada (for the provinces of Quebec
provided by the Ministere des Ressources Naturelles du Quebec, Ontario
provided by OnTAP's Growth and Yield Program of the Ontario Ministry of
Natural Resources, Saskatchewan, Manitoba, New Brunswick, Newfoundland
and Labrador), CTFS (BCI and LTER-Luquillo), Taiwan (Fushan), Cirad
(Paracou with funding by CEBA, ANR-10-LABX-25-01), Cirad, MEFCP and ICRA
(M'Baiki) and Japan. We thank MPI-BGC Jena, who host TRY, and the
international funding networks supporting TRY (IGBP, DIVERSITAS, GLP,
NERC, QUEST, FRB and GIS Climate). G.K. was supported by a Marie Curie
International Outgoing Fellowship within the 7th European Community
Framework Program (Demo-Traits project, no. 299340). The working group
that initiated this synthesis was supported by Macquarie University and
by Australian Research Council through a fellowship to M.W.
NR 129
TC 30
Z9 30
U1 77
U2 265
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 14
PY 2016
VL 529
IS 7585
BP 204
EP U174
DI 10.1038/nature16476
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA7WK
UT WOS:000368015700035
PM 26700807
ER
PT J
AU Aguila, RN
Davis, DR
AF Nunez Aguila, Rayner
Davis, Don R.
TI Antillopsyche sessilis, new genus and species, a new Psychidae
(Lepidoptera: Tineoidea) from Cuba with an unusual larval feeding
behavior
SO ZOOTAXA
LA English
DT Article
DE Arrhenophaninae; Dryadaulidae; larval case; sessile larva; Typhoniinae
AB A new genus and species, Antillopsyche sessilis Nunez & Davis, of Psychidae are described from Cuba, West Indies. The new taxon shares certain features with some members of the subfamily Arrhenophaninae but more with the larvae and the fully winged adult females of other subfamilies of Psychidae. Antillopsyche has been assigned provisionally to the subfamily Typhoniinae based on these similarities. Several aspects of its larval biology are described, including the sessile larval cases and foraging behavior, both unique among the known Psychidae. An undescribed species of Dryadaula Meyrick, 1893 (Dryadaulidae) was found inhabiting the larval cases of A. sessilis, but their ecological relationships remain unclear. Other ecological data for Antillopsyche such as distribution, habitat, and parasitoids are also provided.
C1 [Nunez Aguila, Rayner] Inst Ecol & Sistemat, Subdirecc Colecc Zool & Sistemat, Havana, Cuba.
[Davis, Don R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
RP Aguila, RN (reprint author), Inst Ecol & Sistemat, Subdirecc Colecc Zool & Sistemat, Havana, Cuba.
EM raynernunez75@gmail.com; davisd@si.edu
FU Smithsonian Institution Short Term Visitor Program; Zoological
Collections Management Project of the Institute of Ecology and
Systematics, Havana, Cuba
FX We are grateful to Pedro Lopez and other members of Turquino National
Park staff, Granma province, Cuba, for their help toward the success of
the expeditions. We also thank Elier Fonseca and Alejandro Barro,
Faculty of Biology, Havana University for their help during field work.
This work was partly funded through an award of the Smithsonian
Institution Short Term Visitor Program and the Zoological Collections
Management Project of the Institute of Ecology and Systematics, Havana,
Cuba. We wish to thank Peter Hattenschwiler, Uster, Switzerland, and
Wille Sauter, Illnau, Switzerland, for their comments regarding the
subfamily relationships of Antillopsyche. Vichai Malikul, Young Sohn,
Donald Harvey, and Karolyn Darrow of the Department of Entomology,
Smithsonian Institution, assisted with the illustrations, graphics, and
the preparation of plates used in this publication.
NR 14
TC 0
Z9 0
U1 1
U2 4
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 13
PY 2016
VL 4066
IS 1
BP 52
EP 62
PG 11
WC Zoology
SC Zoology
GA DA6DD
UT WOS:000367891400003
PM 27395529
ER
PT J
AU McCranie, JR
Hedges, SB
AF McCranie, James R.
Hedges, S. Blair
TI Molecular phylogeny and taxonomy of the Epictia goudotii Species complex
(Serpentes: Leptotyphlopidae: Epictinae) in Middle America and northern
South America
SO PEERJ
LA English
DT Article
DE Epictia albifrons; Epictia tenella; Middle America; Epictia goudotii
Species complex; Northern South America; Threadsnakes; Molecular
phylogeny
ID SQUAMATA
AB Here we review the systematics of the threadsnakes of the Epictia goudotii Species complex in Middle and northern South America using external morphology and molecular data. Two species, Epictia goudotii and E. magnamaculata, are currently recognized from that region, but we provide evidence for recognizing, as species, three other nominal forms usually treated as subspecies of E. goudotii: E. ater, E. bakewelli, and E. phenops. Thus, together with E. columbi (Bahamas), we recognize six species in the Epictia goudotii Species complex. Because E. albifrons from northern South America has been confused with E. goudotii in the past, we also briefly discuss the taxonomic status of that species and its apparent close relative E. tenella, which are not members of the E. goudotii complex.
C1 [McCranie, James R.] Smithsonian Inst, Miami, FL USA.
[Hedges, S. Blair] Temple Univ, Ctr Biodivers, Philadelphia, PA 19122 USA.
RP Hedges, SB (reprint author), Temple Univ, Ctr Biodivers, Philadelphia, PA 19122 USA.
EM sbh@temple.edu
NR 68
TC 2
Z9 3
U1 3
U2 6
PU PEERJ INC
PI LONDON
PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND
SN 2167-8359
J9 PEERJ
JI PeerJ
PD JAN 12
PY 2016
VL 4
AR e1551
DI 10.7717/peerj.1551
PG 27
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA8PD
UT WOS:000368066600004
PM 26788430
ER
PT J
AU Hoyer, S
Lopez-Morales, M
Rojo, P
Minniti, D
Adams, ER
AF Hoyer, S.
Lopez-Morales, M.
Rojo, P.
Minniti, D.
Adams, E. R.
TI TraMoS - IV. Discarding the Quick Orbital Decay Hypothesis for
OGLE-TR-113b
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; techniques: photometric; ephemerides; time;
planets and satellites: individual: OGLE-TR-113b
ID IN EXTRASOLAR PLANETS; TIDAL DISSIPATION; TRANSIT; PHOTOMETRY;
CANDIDATES; EVOLUTION; ACCURACY; PROJECT
AB In the context of the Transit Monitoring in the South project, we present nine new transit observations of the exoplanet OGLE-TR-113b observed with the Gemini South, Magellan Baade, Danish-1.54 m and Southern Astrophysical Research telescopes. We perform a homogeneous analysis of these new transits together with 10 literature transits to probe into the potential detection of an orbital decay previously reported for this planet. Our new observations extend the transit monitoring baseline for this system by 6 yr, to a total of more than 13 yr. With our timing analysis we obtained a. (P) over dot = -1.0 +/- 6.0 ms yr(-1), which rejects previous hints of a larger orbital decay for OGLE-TR-113b. With our updated value of (P) over dot we can discard tidal quality factors of Q(star) < 10(5) for its host star. Additionally, we calculate a 1 sigma dispersion of the transit timing variations of 42 s over the 13 yr baseline, which discards additional planets in the system more massive than 0.5-3.0 M-circle plus in 1:2, 5:3, 2:1 and 3:1 Mean Motion Resonances with OGLE-TR-113b. Finally, with the joint analysis of the 19 light curves we update transit parameters, such as the relative semimajor axis a/R-s = 6.44(-0.05)(+0.04), the planet-to-star radius ratio R-p/R-s = 0.14436(-0.00088)(+0.00096), and constrains its orbital inclination to i = 89.27(-0.68)(+0.51) deg.
C1 [Hoyer, S.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Hoyer, S.] Univ la Laguna, Dept Astrofis, E-38206 San Cristobal de la Laguna, Tenerife, Spain.
[Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
[Rojo, P.] Univ Chile, Dept Astron, Santiago, Chile.
[Minniti, D.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Minniti, D.] Vatican Observ, I-00120 Vatican City, Vatican.
[Minniti, D.] Millennium Inst Astrophys, Santiago, RM, Chile.
[Minniti, D.] Pontificia Univ Catolica Chile, Santiago, Chile.
[Adams, E. R.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Hoyer, S (reprint author), Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain.
EM shoyer@iac.es; mlopez-morales@cfa.harvard.edu; projo@das.uchile.cl
RI Rojo, Patricio/I-5765-2016
FU Spanish Ministry of Economy and Competitiveness (MINECO)
[SEV-2011-0187]; Fondecyt [1120299, Anillo ACT1120]; Millennium
Institute of Astropysics MAS from the Ministry of Economy ICM grant
[P07-021-F]; BASAL CATA Center for Astrophysics and Associated
Technologies [PFB-06]
FX SH acknowledges financial support from the Spanish Ministry of Economy
and Competitiveness (MINECO) under the 2011 Severo Ochoa Program
SEV-2011-0187. PR acknowledges Fondecyt #1120299, Anillo ACT1120. DM is
supported by the Millennium Institute of Astropysics MAS from the
Ministry of Economy ICM grant P07-021-F. PR and DM are also supported by
the BASAL CATA Center for Astrophysics and Associated Technologies
PFB-06.
NR 30
TC 2
Z9 2
U1 3
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1334
EP 1340
DI 10.1093/mnras/stv2362
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100014
ER
PT J
AU Zaninoni, E
Bernardini, MG
Margutti, R
Amati, L
AF Zaninoni, E.
Bernardini, M. G.
Margutti, R.
Amati, L.
TI Update on the GRB universal scaling E-X,E-iso-E-gamma,E-iso-E-pk with 10
years of Swift data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; gamma-rays: general; X-rays: general
ID GAMMA-RAY-BURSTS; EXTENDED EMISSION; LIGHT CURVES; E-P,E-I-E-ISO
CORRELATION; PEAK ENERGY; PHOTOSPHERIC EMISSION; AFTERGLOW EMISSION;
COMPLETE SAMPLE; SPIN-DOWN; LONG ONE
AB From a comprehensive statistical analysis of Swift X-ray light curves of gamma-ray bursts (GRBs) collected from 2004 December to the end of 2010, we found a three-parameter correlation between the isotropic energy emitted in the rest-frame 1-10(4) keV energy band during the prompt emission (E-gamma,E-iso), the rest-frame peak of the prompt emission energy spectrum (E-pk), and the X-ray energy emitted in the rest-frame 0.3-30 keV observed energy band (E-X,E- iso), computed excluding the contribution of the flares. In this paper, we update this correlation with the data collected until 2014 June, expanding the sample size with similar to 35 per cent more objects, where the number of short GRBs doubled. With this larger sample, we confirm the existence of a universal correlation that connects the prompt and afterglow properties of long and short GRBs. We show that this correlation does not depend on the X-ray light-curve morphology and that further analysis is necessary to firmly exclude possible biases derived by redshift measurements. In addition, we discuss about the behaviour of the peculiar objects as ultra-long GRBs and we propose the existence of an intermediate group between long and short GRBs. Interestingly, two GRBs with uncertain classification fall into this category. Finally, we discuss the physics underlying this correlation, in the contest of the efficiency of conversion of the prompt gamma-ray emission energy into the kinetic energy of the afterglow, the photospheric model, and the cannonball model.
C1 [Zaninoni, E.] Ctr Brasileiro Pesquisas Fis, ICRANet Rio, BR-22290180 Rio De Janeiro, Brazil.
[Bernardini, M. G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
[Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Amati, L.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-40129 Bologna, Italy.
RP Zaninoni, E (reprint author), Ctr Brasileiro Pesquisas Fis, ICRANet Rio, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, Brazil.
EM elena.zaninoni@gmail.com
FU International Cooperation Program CAPES-ICRANet - CAPES - Brazilian
Federal Agency for Support and Evaluation of Graduate Education;
Ministry of Education of Brazil; T-REX program
FX We thank the anonymous referee for the helpful comments that have
improved this paper. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester. EZ thanks Luca Izzo
and Marco Muccino for sharing their data. EZ acknowledges the support by
the International Cooperation Program CAPES-ICRANet financed by CAPES -
Brazilian Federal Agency for Support and Evaluation of Graduate
Education within the Ministry of Education of Brazil. MGB thanks support
from the T-REX program.
NR 77
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1375
EP 1384
DI 10.1093/mnras/stv2393
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100017
ER
PT J
AU Wittenmyer, RA
Butler, RP
Wang, L
Bergmann, C
Salter, GS
Tinney, CG
Johnson, JA
AF Wittenmyer, R. A.
Butler, R. P.
Wang, L.
Bergmann, C.
Salter, G. S.
Tinney, C. G.
Johnson, J. A.
TI The Pan-Pacific Planet Search III: five companions orbiting giant stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: radial velocities; planetary systems; planets and
satellites: detection
ID SOLAR-TYPE STARS; SUN-LIKE STARS; SPECTROSCOPIC BINARIES; SUBSTELLAR
COMPANIONS; EXOPLANET DETECTION; RADIAL-VELOCITIES; MASS; MULTIPLICITY;
METALLICITY; PARAMETERS
AB We report a new giant planet orbiting the K giant HD 155233, as well as four stellar-mass companions from the Pan-Pacific Planet Search, a Southern hemisphere radial velocity survey for planets orbiting nearby giants and sub-giants. We also present updated velocities and a refined orbit for HD 47205b (7 CMa b), the first planet discovered by this survey. HD 155233b has a period of 885 +/- 63 d, eccentricity e = 0.03 +/- 0.20, and m sin i = 2.0 +/- 0.5 M-Jup. The stellar-mass companions range in m sin i from 0.066 to 0.33 M-circle dot. Whilst HD 104358B falls slightly below the traditional 0.08 M-circle dot hydrogen-burning mass limit, and is hence a brown-dwarf candidate, we estimate only a 50 per cent a priori probability of a truly sub-stellar mass.
C1 [Wittenmyer, R. A.; Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Wang, L.] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China.
[Bergmann, C.] Univ Canterbury, Dept Phys & Astron, Christchurch 8041, New Zealand.
[Salter, G. S.] Aix Marseille Univ, UMR 7326, CNRS, LAM, F-13388 Marseille, France.
[Johnson, J. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wittenmyer, RA (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM rob@phys.unsw.edu.au
RI Butler, Robert/B-1125-2009
NR 59
TC 4
Z9 4
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1398
EP 1405
DI 10.1093/mnras/stv2396
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100019
ER
PT J
AU Reid, B
Ho, S
Padmanabhan, N
Percival, WJ
Tinker, J
Tojeiro, R
White, M
Eisenstein, DJ
Maraston, C
Ross, AJ
Sanchez, AG
Schlegel, D
Sheldon, E
Strauss, MA
Thomas, D
Wake, D
Beutler, F
Bizyaev, D
Bolton, AS
Brownstein, JR
Chuang, CH
Dawson, K
Harding, P
Kitaura, FS
Leauthaud, A
Masters, K
McBride, CK
More, S
Olmstead, MD
Oravetz, D
Nuza, SE
Pan, K
Parejko, J
Pforr, J
Prada, F
Rodriguez-Torres, S
Salazar-Albornoz, S
Samushia, L
Schneider, DP
Scoccola, CG
Simmons, A
Vargas-Magana, M
AF Reid, Beth
Ho, Shirley
Padmanabhan, Nikhil
Percival, Will J.
Tinker, Jeremy
Tojeiro, Rita
White, Martin
Eisenstein, Daniel J.
Maraston, Claudia
Ross, Ashley J.
Sanchez, Ariel G.
Schlegel, David
Sheldon, Erin
Strauss, Michael A.
Thomas, Daniel
Wake, David
Beutler, Florian
Bizyaev, Dmitry
Bolton, Adam S.
Brownstein, Joel R.
Chuang, Chia-Hsun
Dawson, Kyle
Harding, Paul
Kitaura, Francisco-Shu
Leauthaud, Alexie
Masters, Karen
McBride, Cameron K.
More, Surhud
Olmstead, Matthew D.
Oravetz, Daniel
Nuza, Sebastian E.
Pan, Kaike
Parejko, John
Pforr, Janine
Prada, Francisco
Rodriguez-Torres, Sergio
Salazar-Albornoz, Salvador
Samushia, Lado
Schneider, Donald P.
Scoccola, Claudia G.
Simmons, Audrey
Vargas-Magana, Mariana
TI SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy
target selection and large-scale structure catalogues
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmology: observations; (cosmology:) large-scale structure of Universe
ID DIGITAL SKY SURVEY; POWER-SPECTRUM ANALYSIS; LUMINOUS RED GALAXIES;
LOW-REDSHIFT SAMPLE; ACOUSTIC-OSCILLATIONS; GROWTH-RATE; PHOTOMETRIC
SYSTEM; III/BOSS GALAXIES; DISTANCE SCALE; NEUTRINO MASS
AB The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan Digital Sky Survey (SDSS) III project, has provided the largest survey of galaxy redshifts available to date, in terms of both the number of galaxy redshifts measured by a single survey, and the effective cosmological volume covered. Key to analysing the clustering of these data to provide cosmological measurements is understanding the detailed properties of this sample. Potential issues include variations in the target catalogue caused by changes either in the targeting algorithm or properties of the data used, the pattern of spectroscopic observations, the spatial distribution of targets for which redshifts were not obtained, and variations in the target sky density due to observational systematics. We document here the target selection algorithms used to create the galaxy samples that comprise BOSS. We also present the algorithms used to create large-scale structure catalogues for the final Data Release (DR12) samples and the associated random catalogues that quantify the survey mask. The algorithms are an evolution of those used by the BOSS team to construct catalogues from earlier data, and have been designed to accurately quantify the galaxy sample. The code used, designated MKSAMPLE, is released with this paper.
C1 [Reid, Beth; Schlegel, David] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Reid, Beth; Schlegel, David; Beutler, Florian] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Padmanabhan, Nikhil; Parejko, John] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Percival, Will J.; Maraston, Claudia; Thomas, Daniel; Masters, Karen; Pforr, Janine] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Tinker, Jeremy] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Tojeiro, Rita] Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[White, Martin] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA.
[Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ross, Ashley J.] Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Sanchez, Ariel G.; Salazar-Albornoz, Salvador] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Sheldon, Erin] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Wake, David] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Wake, David] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Bizyaev, Dmitry; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey] Apache Point Observ, Sunspot, NM 88349 USA.
[Bizyaev, Dmitry; Oravetz, Daniel; Pan, Kaike] New Mexico State Univ, Sunspot, NM 88349 USA.
[Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle; Olmstead, Matthew D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Chuang, Chia-Hsun; Prada, Francisco; Rodriguez-Torres, Sergio; Salazar-Albornoz, Salvador] Univ Autonoma Madrid, Inst Fis Teor, UAM CSIC, E-28049 Madrid, Spain.
[Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Kitaura, Francisco-Shu] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Leauthaud, Alexie; More, Surhud] Univ Tokyo, UTIAS, Kavli IPMU, Kashiwa, Chiba 2778583, Japan.
[Olmstead, Matthew D.] Kings Coll, Dept Chem & Phys, Wilkes Barre, PA 18711 USA.
[Nuza, Sebastian E.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Pforr, Janine] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Prada, Francisco; Rodriguez-Torres, Sergio] UAM CSIC, E-28049 Madrid, Spain.
[Prada, Francisco] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18080 Granada, Spain.
[Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Salazar-Albornoz, Salvador] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Samushia, Lado] Kansas State Univ, Manhattan, KS 66506 USA.
[Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Scoccola, Claudia G.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Scoccola, Claudia G.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, Argentina.
[Scoccola, Claudia G.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.
[Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
RP Reid, B (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
EM will.percival@port.ac.uk
RI White, Martin/I-3880-2015
OI White, Martin/0000-0001-9912-5070
FU Alfred P. Sloan Foundation; National Science Foundation; US Department
of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the US Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory, Carnegie
Mellon University, University of Florida, the French Participation
Group, the German Participation Group, Harvard University, the Instituto
de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University.
NR 99
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1553
EP 1573
DI 10.1093/mnras/stv2382
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100031
ER
PT J
AU Welikala, N
Bethermin, M
Guery, D
Strandet, M
Aird, KA
Aravena, M
Ashby, MLN
Bothwell, M
Beelen, A
Bleem, LE
de Breuck, C
Brodwin, M
Carlstrom, JE
Chapman, SC
Crawford, TM
Dole, H
Dore, O
Everett, W
Flores-Cacho, I
Gonzalez, AH
Gonzalez-Nuevo, J
Greve, TR
Gullberg, B
Hezaveh, YD
Holder, GP
Holzapfel, WL
Keisler, R
Lagache, G
Ma, J
Malkan, M
Marrone, DP
Mocanu, LM
Montier, L
Murphy, EJ
Nesvadba, NPH
Omont, A
Pointecouteau, E
Puget, JL
Reichardt, CL
Rotermund, KM
Scott, D
Serra, P
Spilker, JS
Stalder, B
Stark, AA
Story, K
Vanderlinde, K
Vieira, JD
Weiss, A
AF Welikala, N.
Bethermin, M.
Guery, D.
Strandet, M.
Aird, K. A.
Aravena, M.
Ashby, M. L. N.
Bothwell, M.
Beelen, A.
Bleem, L. E.
de Breuck, C.
Brodwin, M.
Carlstrom, J. E.
Chapman, S. C.
Crawford, T. M.
Dole, H.
Dore, O.
Everett, W.
Flores-Cacho, I.
Gonzalez, A. H.
Gonzalez-Nuevo, J.
Greve, T. R.
Gullberg, B.
Hezaveh, Y. D.
Holder, G. P.
Holzapfel, W. L.
Keisler, R.
Lagache, G.
Ma, J.
Malkan, M.
Marrone, D. P.
Mocanu, L. M.
Montier, L.
Murphy, E. J.
Nesvadba, N. P. H.
Omont, A.
Pointecouteau, E.
Puget, J. L.
Reichardt, C. L.
Rotermund, K. M.
Scott, D.
Serra, P.
Spilker, J. S.
Stalder, B.
Stark, A. A.
Story, K.
Vanderlinde, K.
Vieira, J. D.
Weiss, A.
TI Probing star formation in the dense environments of z similar to 1
lensing haloes aligned with dusty star-forming galaxies detected with
the South Pole Telescope
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; galaxies: formation; galaxies: statistics; diffuse radiation;
submillimetre: galaxies
ID OPTICALLY SELECTED GALAXIES; HERSCHEL-SPIRE INSTRUMENT; FUTURE LARGE
SURVEYS; DARK-MATTER HALOES; SPT-SZ SURVEY; SUBMILLIMETER GALAXIES;
NUMBER COUNTS; BACKGROUND ANISOTROPIES; CROSS-CORRELATION; REDSHIFT
AB We probe star formation in the environments of massive (similar to 10(13) M-circle dot) dark matter haloes at redshifts of z similar to 1. This star formation is linked to a submillimetre clustering signal which we detect in maps of the Planck High Frequency Instrument that are stacked at the positions of a sample of high redshift (z > 2) strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope (SPT) 2500 deg(2) survey. The clustering signal has submillimetre colours which are consistent with the mean redshift of the foreground lensing haloes (z similar to 1). We report a mean excess of star formation rate (SFR) compared to the field, of (2700 +/- 700) M-circle dot yr(-1) from all galaxies contributing to this clustering signal within a radius of 3.5 arcmin from the SPT DSFGs. The magnitude of the Planck excess is in broad agreement with predictions of a current model of the cosmic infrared background. The model predicts that 80 per cent of the excess emission measured by Planck originates from galaxies lying in the neighbouring haloes of the lensing halo. Using Herschel maps of the same fields, we find a clear excess, relative to the field, of individual sources which contribute to the Planck excess. The mean excess SFR compared to the field is measured to be (370 +/- 40) M-circle dot yr(-1) per resolved, clustered source. Our findings suggest that the environments around these massive z similar to 1 lensing haloes host intense star formation out to about 2 Mpc. The flux enhancement due to clustering should also be considered when measuring flux densities of galaxies in Planck data.
C1 [Welikala, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Bethermin, M.; de Breuck, C.; Gullberg, B.] European So Observ, D-85748 Garching, Germany.
[Guery, D.; Beelen, A.; Dole, H.; Lagache, G.; Nesvadba, N. P. H.; Puget, J. L.; Serra, P.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aird, K. A.] Univ Chicago, Chicago, IL 60637 USA.
[Aravena, M.] Univ Diego Portales, Nucl Astron, Fac Ingn, Santiago, Chile.
[Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bothwell, M.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England.
[Bleem, L. E.; Carlstrom, J. E.; Crawford, T. M.; Mocanu, L. M.; Story, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Mocanu, L. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.; Rotermund, K. M.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada.
[Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, O.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Everett, W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Everett, W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Flores-Cacho, I.; Montier, L.; Pointecouteau, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Flores-Cacho, I.; Montier, L.; Pointecouteau, E.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Gonzalez-Nuevo, J.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Gonzalez-Nuevo, J.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Hezaveh, Y. D.; Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Omont, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Welikala, N (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
EM niraj.welikala@physics.ox.ac.uk
RI Gonzalez-Nuevo, Joaquin/I-3562-2014;
OI Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Scott,
Douglas/0000-0002-6878-9840; De Breuck, Carlos/0000-0002-6637-3315
FU National Science Foundation [PLR-1248097]; NSF Physics Frontier Center
[PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF
947]; US National Science Foundation [AST-1312950]; ESA Member States;
NASA; ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR
(Italy); INAF (Italy); NASA (USA); DoE (USA); Beecroft Institute for
Particle Astrophysics and Cosmology; Centre National d'Etudes Spatiales
(CNES); National Aeronautics and Space Administration; International Max
Planck Research School (IMPRS) for Astronomy and Astrophysics at the
Universities of Bonn and Cologne; Spanish CSIC; European Social Fund;
Spanish Ministerio de Ciencia e Innovacion [AYA2012-39475-C02-01];
Consolider-Ingenio [CSD2010-00064]; [ANR-11-BS56-015]
FX We thank the anonymous referee for valuable comments. The South Pole
Telescope is supported by the National Science Foundation through grant
PLR-1248097. Partial support is also provided by the NSF Physics
Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological
Physics at the University of Chicago, the Kavli Foundation, and the
Gordon and Betty Moore Foundation grant GBMF 947. This paper is based on
work supported by the US National Science Foundation under grant no.
AST-1312950. Based on observations obtained with Planck
(http://www.esa.int/Planck), an ESA science mission with instruments and
contributions directly funded by ESA Member States, NASA, and Canada.
The development of Planck has been supported by: ESA; CNES and
CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE
(USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and
CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark);
SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); and PRACE (EU). A description of the Planck Collaboration
and a list of its members, including the technical or scientific
activities in which they have been involved, can be found at
http://www.rssd.esa.int/index.php?project=PLANCK&page=PlanckCollaboratio
n. This paper makes use of the following ALMA data: ADS/JAO.
ALMA#2011.0.00957.S. ALMA is a partnership of ESO (representing its
member states), NSF (USA), and NINS (Japan), together with NRC (Canada)
and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile.
The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. APEX
is a collaboration between the Max-Planck-Institut fur Radioastronomie,
the European Southern Observatory, and the Onsala Space Observatory.
This work is based in part on observations made with Herschel, a
European Space Agency Cornerstone Mission with significant participation
by NASA, and supported through an award issued by JPL/Caltech for
OT2_jvieira_5. NW acknowledges support from the Beecroft Institute for
Particle Astrophysics and Cosmology and previous support from the Centre
National d'Etudes Spatiales (CNES). Part of the research described in
this paper was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. MS was supported for this research through a
stipend from the International Max Planck Research School (IMPRS) for
Astronomy and Astrophysics at the Universities of Bonn and Cologne. IF-C
acknowledges the support of grant ANR-11-BS56-015. JG-N acknowledges
financial support from the Spanish CSIC for a JAE-DOC fellowship,
cofunded by the European Social Fund, by the Spanish Ministerio de
Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010,
CSD2010-00064, projects. NW thanks B. Partridge, J. Delabrouille, D.
Harrison, and P. Vielva for useful comments.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1629
EP 1646
DI 10.1093/mnras/stv2302
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100036
ER
PT J
AU Runnoe, JC
Cales, S
Ruan, JJ
Eracleous, M
Anderson, SF
Shen, Y
Green, PJ
Morganson, E
LaMassa, S
Greene, JE
Dwelly, T
Schneider, DP
Merloni, A
Georgakakis, A
Roman-Lopes, A
AF Runnoe, Jessie C.
Cales, Sabrina
Ruan, John J.
Eracleous, Michael
Anderson, Scott F.
Shen, Yue
Green, Paul J.
Morganson, Eric
LaMassa, Stephanie
Greene, Jenny E.
Dwelly, Tom
Schneider, Donald P.
Merloni, Andrea
Georgakakis, Antonis
Roman-Lopes, A.
TI Now you see it, now you don't: the disappearing central engine of the
quasar J1011+5442
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; galaxies: active; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; TIDAL DISRUPTION EVENTS;
BROAD-LINE EMISSION; BLACK-HOLE MASSES; DATA RELEASE; SEYFERT-GALAXIES;
SPECTROSCOPIC SURVEY; HOST GALAXIES; LIGHT CURVES
AB We report the discovery of a new 'changing-look' quasar, SDSS J101152.98+544206.4, through repeat spectroscopy from the Time Domain Spectroscopic Survey. This is an addition to a small but growing set of quasars whose blue continua and broad optical emission lines have been observed to decline by a large factor on a time-scale of approximately a decade. The 5100 angstrom monochromatic continuum luminosity of this quasar drops by a factor of > 9.8 in a rest-frame time interval of < 9.7 yr, while the broad Ha luminosity drops by a factor of 55 in the same amount of time. The width of the broad Ha line increases in the dim state such that the black hole mass derived from the appropriate single-epoch scaling relation agrees between the two epochs within a factor of 3. The fluxes of the narrow emission lines do not appear to change between epochs. The light curve obtained by the Catalina Sky Survey suggests that the transition occurs within a rest-frame time interval of approximately 500 d. We examine three possible mechanisms for this transition suggested in the recent literature. An abrupt change in the reddening towards the central engine is disfavoured by the substantial difference between the time-scale to obscure the central engine and the observed time-scale of the transition. A decaying tidal disruption flare is consistent with the decay rate of the light curve but not with the prolonged bright state preceding the decay; nor can this scenario provide the power required by the luminosities of the emission lines. An abrupt drop in the accretion rate on to the supermassive black hole appears to be the most plausible explanation for the rapid dimming.
C1 [Runnoe, Jessie C.; Eracleous, Michael; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cales, Sabrina] Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA.
[Cales, Sabrina] Univ Concepcion, Fac Phys & Math Sci, Dept Astron, Concepcion, Chile.
[Ruan, John J.; Anderson, Scott F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA.
[Shen, Yue] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Green, Paul J.; Morganson, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Greene, Jenny E.] Princeton Univ Observ, Princeton, NJ 08544 USA.
[Dwelly, Tom; Merloni, Andrea; Georgakakis, Antonis] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
[Roman-Lopes, A.] Univ La Serena, Fac Ciencias, Dept Fis & Astron, La Serena 1200, Chile.
RP Runnoe, JC (reprint author), Penn State Univ, Inst Gravitat & Cosmos, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM jcr26@psu.edu
RI Georgakakis, Antonis/K-4457-2013
FU DIULS Regular project [PR15143]; Alfred P. Sloan Foundation; Center for
High-Performance Computing at the University of Utah; SDSS Collaboration
including the Brazilian Participation Group; Carnegie Institution for
Science; Carnegie Mellon University; Chilean Participation Group;
Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de
Canarias; Johns Hopkins University; Kavli Institute for the Physics and
Mathematics of the Universe (IPMU) / University of Tokyo; Lawrence
Berkeley National Laboratory; Leibniz Institut fr Astrophysik Potsdam
(AIP); Max-Planck-Institut fr Astrophysik (MPA, Garching);
Max-Planck-Institut fr Extraterrestrische Physik (MPE);
Max-Planck-Institut fr Astronomie (MPIA, Heidelberg); National
Astronomical Observatory of China; New Mexico State University; New York
University; University of Notre Dame; Observatrio Nacional do Brasil;
Ohio State University; Pennsylvania State University; Shanghai
Astronomical Observatory; United Kingdom Participation Group;
Universidad Nacional Autnoma de Mexico; University of Arizona;
University of Colorado Boulder; University of Portsmouth; University of
Utah; University of Washington; University of Wisconsin; Vanderbilt
University; Yale University; National Aeronautics and Space
Administration [NNG05GF22G]; US National Science Foundation
[AST-0909182]; National Aeronautics and Space Administration at MIT
Lincoln Laboratory under Air Force [FA8721-05-C-0002]
FX We thank the referee, Benjamin Shappee, for helpful comments and
suggestions. ARL acknowledges partial financial support from the DIULS
Regular project PR15143.; Funding for the Sloan Digital Sky Survey IV
has been provided by the Alfred P. Sloan Foundation and the
Participating Institutions. SDSS-IV acknowledges support and resources
from the Center for High-Performance Computing at the University of
Utah. The SDSS web site is www.sdss.org.; SDSS-IV is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS Collaboration including the Brazilian Participation Group,
Carnegie Institution for Science, Carnegie Mellon University, the
Chilean Participation Group, Harvard-Smithsonian Center for
Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins
University, Kavli Institute for the Physics and Mathematics of the
Universe (IPMU) / University of Tokyo, Lawrence Berkeley National
Laboratory, Leibniz Institut fr Astrophysik Potsdam (AIP),
Max-Planck-Institut fr Astrophysik (MPA, Garching), Max-Planck-Institut
fr Extraterrestrische Physik (MPE), Max-Planck-Institut fr Astronomie
(MPIA, Heidelberg), National Astronomical Observatory of China, New
Mexico State University, New York University, University of Notre Dame,
Observatrio Nacional do Brasil, The Ohio State University, Pennsylvania
State University, Shanghai Astronomical Observatory, United Kingdom
Participation Group, Universidad Nacional Autnoma de Mexico, University
of Arizona, University of Colorado Boulder, University of Portsmouth,
University of Utah, University of Washington, University of Wisconsin,
Vanderbilt University, and Yale University.; The CSS survey is funded by
the National Aeronautics and Space Administration under Grant No.
NNG05GF22G issued through the Science Mission Directorate Near-Earth
Objects Observations Program. The CRTS survey is supported by the US
National Science Foundation under grants AST-0909182.; The LINEAR
program is funded by the National Aeronautics and Space Administration
at MIT Lincoln Laboratory under Air Force Contract FA8721-05-C-0002.
Opinions, interpretations, conclusions, and recommendations are those of
the authors and are not necessarily endorsed by the United States
Government.
NR 93
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1691
EP 1701
DI 10.1093/mnras/stv2385
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100041
ER
PT J
AU Watson, LC
Martini, P
Lisenfeld, U
Boker, T
Schinnerer, E
AF Watson, Linda C.
Martini, Paul
Lisenfeld, Ute
Boeker, Torsten
Schinnerer, Eva
TI Testing the molecular-hydrogen Kennicutt-Schmidt law in the low-density
environments of extended ultraviolet disc galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE H II regions; ISM: molecules; galaxies: ISM; galaxies: star formation
ID STAR-FORMATION LAW; CO-TO-H-2 CONVERSION FACTOR; EXTREME OUTER REGIONS;
INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; H II REGIONS; NEARBY
GALAXIES; SPIRAL GALAXIES; FORMING GALAXIES; LOCAL UNIVERSE
AB Studying star formation beyond the optical radius of galaxies allows us to test empirical relations in extreme conditions with low average gas density and low molecular fraction. Previous studies discovered galaxies with extended ultraviolet (XUV) discs, which often contain star-forming regions with lower H alpha-to-far-UV (FUV) flux ratios compared to inner disc star-forming regions. However, most previous studies lack measurements of molecular gas, which is presumably the component of the interstellar medium out of which stars form. We analysed published CO measurements and upper limits for 15 star-forming regions in the XUV or outer disc of three nearby spiral galaxies and a new CO upper limit from the IRAM (Institut de Radioastronomie Millim ' etrique) 30m telescope in one star-forming region at r = 3.4r(25) in the XUV disc of NGC 4625. We found that the star-forming regions are in general consistent with the same molecular-hydrogen Kennicutt-Schmidt law that applies within the optical radius, independent of whether we used H alpha or FUV as the star formation rate (SFR) tracer. However, a number of the CO detections are significantly offset towards higher SFR surface density for their molecular-hydrogen surface density. Deeper CO data may enable us to use the presence or absence of molecular gas as an evolutionary probe to break the degeneracy between age and stochastic sampling of the initial mass function as the explanation for the low H alpha-to-FUV flux ratios in XUV discs.
C1 [Watson, Linda C.] European So Observ, Santiago 19001, Chile.
[Watson, Linda C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martini, Paul] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Martini, Paul] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Lisenfeld, Ute] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain.
[Boeker, Torsten] European Space Agcy STScI, Baltimore, MD 21218 USA.
[Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Watson, LC (reprint author), European So Observ, Alonso de Cordova 3107, Santiago 19001, Chile.
EM lwatson@eso.org
RI Lisenfeld, Ute/A-1637-2015;
OI Lisenfeld, Ute/0000-0002-9471-5423; Schinnerer, Eva/0000-0002-3933-7677
FU Spanish Ministerio de Ciencia y Educacion [AYA2011-24728]; Junta de
Andalucia (Spain) [FQM108]; INSU/CNRS (France); MPG (Germany); IGN
(Spain); NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]
FX We thank Armando Gil de Paz for his advice throughout the project,
Andreas Schruba for sharing his CO(2-1) radial profile, Annette Ferguson
for sharing her Ha image of NGC 6946, Jonathan Braine for sharing his CO
line intensities for NGC 4414, and the referee for comments that
improved this work. UL has been supported by the research projects
AYA2011-24728 from the Spanish Ministerio de Ciencia y Educacion and the
Junta de Andalucia (Spain) grants FQM108. This work is based on
observations carried out with the IRAM 30m Telescope. IRAM is supported
by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This work made
use of HERACLES, 'The HERA CO-Line Extragalactic Survey' (Leroy et al.
2009). Some of the data presented in this paper were obtained from the
MAST. STScI is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX09AF08G and by other grants and contracts. This research has made use
of the NASA/IPAC Extragalactic Database which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the NASA.
NR 82
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 1807
EP 1818
DI 10.1093/mnras/stv2412
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100050
ER
PT J
AU Mashian, N
Oesch, PA
Loeb, A
AF Mashian, Natalie
Oesch, Pascal A.
Loeb, Abraham
TI An empirical model for the galaxy luminosity and star formation rate
function at high redshift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; galaxies: luminosity function, mass function;
cosmology: theory
ID ULTRA-DEEP-FIELD; LYMAN-BREAK GALAXIES; SIMILAR-TO 8; FORMATION RATE
DENSITY; ULTRAVIOLET LUMINOSITY; FORMING GALAXIES; INTERGALACTIC MEDIUM;
COSMIC REIONIZATION; WFC3/IR OBSERVATIONS; IONIZING EMISSIVITY
AB Using the most recent measurements of the ultraviolet (UV) luminosity functions (LFs) and dust estimates of early galaxies, we derive updated dust-corrected star formation rate functions (SFRFs) at z similar to 4-8, which we model to predict the evolution to higher redshifts, z > 8. We employ abundance matching techniques to calibrate a relation between galaxy star formation rate (SFR) and host halo mass M-h by mapping the shape of the observed SFRFs at z UV 4-8 to that of the halo mass function. The resulting scaling law remains roughly constant over this redshift range. We apply the average SFR-M-h relation to reproduce the observed SFR functions at 4 less than or similar to z less than or similar to 8 and also derive the expected UV LFs at higher redshifts. At z similar to 9 and z similar to 10 these model LFs are in excellent agreement with current observed estimates. Our predicted number densities and UV LFs at z > 10 indicate that James Webb Space Telescope will be able to detect galaxies out to z similar to 15 with an extensive treasury sized program. We also derive the redshift evolution of the star formation rate density (SFRD) and associated reionization history by galaxies. Models which integrate down to the current HUDF12/XDF detection limit (M-UV similar to -17.7 mag) result in a SFRD that declines as (1 + z)(-10.4 +/- 0.3) at high redshift and fail to reproduce the observed cosmic microwave background electron scattering optical depth, tau similar or equal to 0.066, to within 1 sigma. On the other hand, we find that the inclusion of galaxies with SFRs well below the current detection limit (M-UV < -5.7 mag) leads to a fully reionized universe by z similar to 6.5 and an optical depth of tau similar or equal to 0.054, consistent with the recently derived Planck value at the 1 sigma level.
C1 [Mashian, Natalie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Oesch, Pascal A.] Yale Univ, Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA.
[Oesch, Pascal A.] Yale Univ, Dept Astron, Ctr Astron & Astrophys, New Haven, CT 06520 USA.
RP Mashian, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nmashian@physics.harvard.edu
OI Oesch, Pascal/0000-0001-5851-6649
FU NSF [AST-1312034]; National Science Foundation [DGE1144152]
FX We thank R. Smit and R. Bouwens for helpful discussions regarding the
SFRF measurements and for comments on an earlier version of this
manuscript. This work was supported in part by NSF grant AST-1312034.
This material is based upon work supported by the National Science
Foundation Graduate Research Fellowship under Grant No. DGE1144152. Any
opinion, findings, and conclusions or recommendations expressed in this
material are those of the authors and do not necessarily reflect the
views of the National Science Foundation.
NR 97
TC 13
Z9 13
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 11
PY 2016
VL 455
IS 2
BP 2101
EP 2109
DI 10.1093/mnras/stv2469
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TN
UT WOS:000368007100072
ER
PT J
AU Cleeves, LI
AF Cleeves, L. Ilsedore
TI MULTIPLE CARBON MONOXIDE SNOW. LINES IN DISKS SCULPTED BY RADIAL DRIFT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; astrochemistry; stars: pre-main sequence
ID PROTOPLANETARY DISKS; INTERSTELLAR GRAINS; TRANSITION DISK; DUST; CO;
ICE; EVOLUTION; GAS; DESORPTION; DENSITY
AB Observations of protoplanetary disks suggest that the gas and dust follow significantly different radial distributions. This finding can be theoretically explained by a combination of radial drift and gas drag of intermediate-sized dust grains. Using a simple parametric model to approximate the different distributions of the gas and dust components, we calculate and examine the impact of radial drift on the global dust temperature structure. We find that the removal of large grains beyond the "truncation radius" allows this region to become significantly warmer from reprocessed stellar radiation shining down from the disk upper layers, increasing the outer disk temperature by similar to 10%-30%. This change is sufficient to raise the local temperature to a value exceeding the CO desorption temperature. These findings imply that the disk density structures induced by radial drift are able to create multiple CO snow. lines. The inner disk CO is in the gas phase, freezing out near the classical snow. line at R similar to 20-40 AU. Moving outward, the CO sublimates once again beyond the truncation radius (80 AU in our models) and subsequently re-freezes out at sufficiently large stellar distances. beyond R greater than or similar to 130-200 AU. We find that thermal desorption of CO in the outer disk becomes competitive with external UV photodesorption and that this additional transition from solid state CO to the gas. phase has significant implications for the C/O ratio in the outer disk.
C1 [Cleeves, L. Ilsedore] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Cleeves, LI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Cleeves, L. Ilsedore/0000-0003-2076-8001
FU NASA - Space Telescope Science Institute [HST-HF2-51356.001-A]; NASA
[NAS 5-26555]
FX The author is grateful to the anonymous referee whose helpful comments
improved this paper. The author also thanks Karin Oberg, David Wilner,
Ryan Loomis, and Andrea Isella for helpful discussions. L.I.C.
acknowledges the support of NASA through Hubble Fellowship grant
HST-HF2-51356.001-A awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555.
NR 39
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2016
VL 816
IS 2
AR L21
DI 10.3847/2041-8205/816/2/L21
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AK
UT WOS:000369370500003
ER
PT J
AU Fayolle, EC
Balfe, J
Loomis, R
Bergner, J
Graninger, D
Rajappan, M
Ouml;berg, KI
AF Fayolle, Edith C.
Balfe, Jodi
Loomis, Ryan
Bergner, Jennifer
Graninger, Dawn
Rajappan, Mahesh
Oeberg, Karin I.
TI N-2 AND CO DESORPTION ENERGIES FROM WATER ICE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: molecules; methods: laboratory:
solid state; molecular data; molecular processes
ID PROTOPLANETARY DISKS; INTERSTELLAR ICES; CIRCUMSTELLAR DISKS;
PROTOSTELLAR CORES; SOLAR-SYSTEM; CHEMISTRY; PHOTODESORPTION; MOLECULES;
EVOLUTION; ANALOGS
AB The relative desorption energies of CO and N-2 are key to interpretations of observed interstellar CO and N-2 abundance patterns, including the well-documented CO and N2H+ anti-correlations in disks, protostars, and molecular cloud cores. Based on laboratory experiments on pure CO and N-2 ice desorption, the difference between CO and N-2 desorption energies is small; the N-2-to-CO desorption energy ratio is 0.93 +/- 0.03. Interstellar ices are not pure, however, and in this study we explore the effect of water ice on the desorption energy ratio of the two molecules. We present temperature programmed desorption experiments of different coverages of (CO)-C-13 and N-15(2) on porous and compact amorphous water ices and, for reference, of pure ices. In all experiments, 15N(2) desorption begins a few degrees before the onset of (CO)-C-13 desorption. The N-15(2) and (CO)-C-13 energy barriers are 770 and 866 K for the pure ices, 1034-1143 K and 1155-1298 K for different submonolayer coverages on compact water ice, and 1435 and 1575 K for similar to 1 ML of ice on top of porous water ice. For all equivalent experiments, the N-2-to-CO desorption energy ratio is consistently 0.9. Whenever CO and N-2 ice reside in similar ice environments (e.g., experience a similar degree of interaction with water ice) their desorption temperatures should thus be within a few degrees of one another. A smaller N-2-to-CO desorption energy ratio may be present in interstellar and circumstellar environments if the average CO ice molecules interacts more with water ice compared to the average N-2 molecules.
C1 [Fayolle, Edith C.; Balfe, Jodi; Loomis, Ryan; Bergner, Jennifer; Graninger, Dawn; Rajappan, Mahesh; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Fayolle, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Rubicon fellowship - Netherlands Organisation for Scientific Research
(NWO) [680-50-1302]; Alfred P. Sloan Foundation; Packard Foundation
FX The authors are grateful to the referee for comments and suggestions
that greatly improved the manuscript. E.C.F. is supported by a Rubicon
fellowship (680-50-1302), awarded by the Netherlands Organisation for
Scientific Research (NWO). K.I.O. acknowledges funding from the Alfred
P. Sloan Foundation, and the Packard Foundation.
NR 41
TC 6
Z9 6
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2016
VL 816
IS 2
AR L28
DI 10.3847/2041-8205/816/2/L28
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AK
UT WOS:000369370500010
ER
PT J
AU Liu, HB
Galvan-Madrid, R
Vorobyov, EI
Kospal, A
Rodriguez, LF
Dunham, MM
Hirano, N
Henning, T
Takami, M
Dong, RB
Hashimoto, J
Hasegawa, Y
Carrasco-Gonzalez, C
AF Liu, Hauyu Baobab
Galvan-Madrid, Roberto
Vorobyov, Eduard I.
Kospal, Agnes
Rodriguez, Luis F.
Dunham, Michael M.
Hirano, Naomi
Henning, Thomas
Takami, Michihiro
Dong, Ruobing
Hashimoto, Jun
Hasegawa, Yasuhiro
Carrasco-Gonzalez, Carlos
TI ABSENCE OF SIGNIFICANT COOL DISKS IN YOUNG STELLAR OBJECTS EXHIBITING
REPETITIVE OPTICAL OUTBURSTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: formation
ID ORION-NEBULA-CLUSTER; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS;
STAR-FORMATION; TAURUS-AURIGA; SUBMILLIMETER ARRAY; MOLECULAR CLOUD;
ACCRETION; EVOLUTION; CONTINUUM
AB We report Submillimeter Array 1.3 mm high angular resolution observations toward the four EXor-type outbursting young stellar objects VY Tau, V1118 Ori, V1143 Ori, and NY Ori. The data mostly show low dust masses Mdust in the associated circumstellar disks. Among the sources, NY Ori possesses a relatively massive disk with M-dust similar to 9 x 10(-4) M-circle dot. V1118 Ori has a marginal detection equivalent to M-dust similar to 6 x 10(-5) M-circle dot. V1143 Ori has a non-detection also equivalent to M-dust < 6 x 10(-5) M-circle dot. For the nearest source, VY Tau, we get a surprising non-detection that provides a stringent upper limit M-dust < 6 x 10(-6) M-circle dot. We interpret our findings as suggesting that the gas and dust reservoirs that feed the short-duration, repetitive optical outbursts seen in some EXors may be limited to the small-scale, innermost region of their circumstellar disks. This hot dust may have escaped our detection limits. Follow-up, more sensitive millimeter observations are needed to improve our understanding of the triggering mechanisms of EXor-type outbursts.
C1 [Liu, Hauyu Baobab; Hirano, Naomi; Takami, Michihiro; Dong, Ruobing] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
[Liu, Hauyu Baobab] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Galvan-Madrid, Roberto; Rodriguez, Luis F.; Carrasco-Gonzalez, Carlos] UNAM, Inst Radioastron & Astrofis, AP 3-72, Morelia 58089, Michoacan, Mexico.
[Vorobyov, Eduard I.] Univ Vienna, Dept Astrophys, Tuerkenschanzstr 17, A-1180 Vienna, Austria.
[Vorobyov, Eduard I.] Southern Fed Univ, Inst Phys Res, Rostov Na Donu 344090, Russia.
[Kospal, Agnes] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.
[Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
[Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Dong, Ruobing] Univ Calif Berkeley, Dept Astron, 147 Mar Ave, Berkeley, CA 94708 USA.
[Hashimoto, Jun] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Hasegawa, Yasuhiro] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.; Liu, HB (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM baobabyoo@gmail.com
FU ASIAA; Momentum grant of the MTA CSFK Lendulet Disk Research Group;
Russian Ministry of Education and Science [3.961.2014/K]; RFBR
[14-02-00719]; Submillimeter Array through an SMA Postdoctoral
Fellowship; JPL/Caltech; MOST [104-2119-M-001-018]; [UNAM-DGAPA-PAPIIT
IA101715]
FX H.B.L. thanks the support from ASIAA and the SMA staff. H.B.L. thanks T.
Muto and S. Hirose for useful discussions. This research was done with
the support of program UNAM-DGAPA-PAPIIT IA101715. This work was
supported by the Momentum grant of the MTA CSFK Lendulet Disk Research
Group. E.I.V. acknowledges the support from the Russian Ministry of
Education and Science Grant 3.961.2014/K and RFBR grant 14-02-00719.
M.M.D. acknowledges support from the Submillimeter Array through an SMA
Postdoctoral Fellowship. Y.H. is supported by JPL/Caltech. We
acknowledge the MOST grant 104-2119-M-001-018.
NR 48
TC 3
Z9 3
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2016
VL 816
IS 2
AR L29
DI 10.3847/2041-8205/816/2/L29
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AK
UT WOS:000369370500011
ER
PT J
AU Ballard, S
Johnson, JA
AF Ballard, Sarah
Johnson, John Asher
TI THE KEPLER DICHOTOMY AMONG THE M DWARFS: HALF OF SYSTEMS CONTAIN FIVE OR
MORE COPLANAR PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems
ID HUBBLE-SPACE-TELESCOPE; SUPER-EARTH GJ1214B; EXOPLANET GJ 1214B;
LOW-MASS; TRANSMISSION SPECTRUM; SOLAR NEIGHBORHOOD; HABITABLE ZONE;
COOL STARS; MULTIPLICITY; II.
AB We present a statistical analysis of the Kepler M dwarf planet hosts, with a particular focus on the fractional number of systems hosting multiple transiting planets. We manufacture synthetic planetary systems within a range of planet multiplicity and mutual inclination for comparison to the Kepler yield. Similarly to studies of Kepler exoplanetary systems around more massive stars, we report that the number of singly transiting planets found by Kepler is too high to be consistent with a single population of multi-planet systems, a finding that cannot be attributed to selection biases. To account for the excess singleton planetary systems we adopt a mixture model and find that 53 +/- 10% of planetary systems are either single or contain multiple planets with large mutual inclinations. The other 47 +/- 10% of systems contain 7.5(-1.5)(+0.5) planets with mutual inclinations of 2.degrees 0 +/- 1.degrees 3. This mutual inclination range is consistent with studies of transit durations within multiply transiting systems. The mixture model is preferred 8:1 to a model with only one architecture. Thus, we find that the so-called "Kepler dichotomy" holds for planets orbiting M dwarfs as well as Sun-like stars.
C1 [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA.
[Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ballard, S (reprint author), Univ Washington, Seattle, WA 98195 USA.
EM sarahba@uw.edu
NR 70
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Z9 8
U1 2
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 66
DI 10.3847/0004-637X/816/2/66
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500018
ER
PT J
AU Brightman, M
Harrison, F
Walton, DJ
Fuerst, F
Hornschemeier, A
Zezas, A
Bachetti, M
Grefenstette, B
Ptak, A
Tendulkar, S
Yukita, M
AF Brightman, Murray
Harrison, Fiona
Walton, Dominic J.
Fuerst, Felix
Hornschemeier, Ann
Zezas, Andreas
Bachetti, Matteo
Grefenstette, Brian
Ptak, Andrew
Tendulkar, Shriharsh
Yukita, Mihoko
TI SPECTRAL AND TEMPORAL PROPERTIES OF THE ULTRA-LUMINOUS X-RAY PULSAR IN
M82 FROM 15 YEARS OF CHANDRA OBSERVATIONS AND ANALYSIS OF THE PULSED
EMISSION USING NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M82); stars: neutron; X-rays: binaries
ID ACCRETING NEUTRON-STAR; XMM-NEWTON; GRO J1744-28; SOFT EXCESS;
BROAD-BAND; GALAXY M82; DISCOVERY; X-1; J095551+6940.8; POPULATION
AB The recent discovery by Bachetti et al. of a pulsar in M82 that can reach luminosities of up to 10(40) erg s(-1), a factor of similar to 100 times the Eddington luminosity for a 1.4 M-circle dot compact object, poses a challenge for accretion physics. In order to better understand the nature of this source and its duty cycle, and in light of several physical models that have been subsequently published, we conduct a spectral and temporal analysis of the 0.5-8 keV X-ray emission from this source from 15 years of Chandra observations. We analyze 19 ACIS observations where the point-spread function (PSF) of the pulsar is not contaminated by nearby sources. We fit the Chandra spectra of the pulsar with a power-law model and a disk blackbody model, subjected to interstellar absorption in M82. We carefully assess for the effect of pile-up in our observations, where four observations have a pile-up fraction of >10%, which we account for during spectral modeling with a convolution model. When fitted with a power-law model, the average photon index when the source is at high luminosity (L-X > 10(39) erg s(-1)) is Gamma = 1.33 +/- 0.15. For the disk blackbody model, the average temperature is T-in = 3.24 +/- 0.65 keV, the spectral shape being consistent with other luminous X-ray pulsars. We also investigated the inclusion of a soft excess component and spectral break, finding that the spectra are also consistent with these features common to luminous X-ray pulsars. In addition, we present spectral analysis from NuSTAR over the 3-50 keV range where we have isolated the pulsed component. We find that the pulsed emission in this band is best fit by a power-law with a high-energy cutoff, where Gamma = 0.6 +/- 0.3 and E-C = 14(-3)(+5) KeV. While the pulsar has previously been identified as a transient, we find from our longer-baseline study that it has been remarkably active over the 15-year period, where for 9/19 (47%) observations that we analyzed, the pulsar appears to be emitting at a luminosity in excess of 10(39) erg s(-1), greater than 10 times its Eddington limit.
C1 [Brightman, Murray; Harrison, Fiona; Walton, Dominic J.; Fuerst, Felix; Grefenstette, Brian; Tendulkar, Shriharsh] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Walton, Dominic J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hornschemeier, Ann; Ptak, Andrew; Yukita, Mihoko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hornschemeier, Ann; Ptak, Andrew; Yukita, Mihoko] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Zezas, Andreas] Univ Crete, Dept Phys, Iraklion, Greece.
[Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zezas, Andreas] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece.
[Bachetti, Matteo] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
RP Brightman, M (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA.
RI Yukita, Mihoko/E-4135-2017; Zezas, Andreas/C-7543-2011
OI Zezas, Andreas/0000-0001-8952-676X
FU NASA; European Research Council under the European Union's Seventh
Framework Programme (FP)/ERC [617001]
FX This work made significant use of archival observations made by the
Chandra X-ray observatory, for which we thank the builders and
operators, as well as the software package CIAO. The data were obtained
from the High Energy Astrophysics Science Archive Research Center
(HEASARC), which is a service of the Astrophysics Science Division at
NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian
Astrophysical Observatory. This work also made use of data from the
NuSTAR mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by NASA. We thank
the NuSTAR Operations, Software, and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA). A.Z. acknowledges funding from the
European Research Council under the European Union's Seventh Framework
Programme (FP/2007-2013)/ERC grant agreement No. 617001.
NR 43
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U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 60
DI 10.3847/0004-637X/816/2/60
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500012
ER
PT J
AU Gettel, S
Charbonneau, D
Dressing, CD
Buchhave, LA
Dumusque, X
Vanderburg, A
Bonomo, AS
Malavolta, L
Pepe, F
Cameron, AC
Latham, DW
Udry, S
Marcy, GW
Isaacson, H
Howard, AW
Davies, GR
Aguirre, VS
Kjeldsen, H
Bedding, TR
Lopez, E
Affer, L
Cosentino, R
Figueira, P
Fiorenzano, AFM
Harutyunyan, A
Johnson, JA
Lopez-Morales, M
Lovis, C
Mayor, M
Micela, G
Molinari, E
Motalebi, F
Phillips, DF
Piotto, G
Queloz, D
Rice, K
Sasselov, D
Segransan, D
Sozzetti, A
Watson, C
Basu, S
Campante, TL
Christensen-Dalsgaard, J
Kawaler, SD
Metcalfe, TS
Handberg, R
Lund, MN
Lundkvist, MS
Huber, D
Chaplin, WJ
AF Gettel, Sara
Charbonneau, David
Dressing, Courtney D.
Buchhave, Lars A.
Dumusque, Xavier
Vanderburg, Andrew
Bonomo, Aldo S.
Malavolta, Luca
Pepe, Francesco
Cameron, Andrew Collier
Latham, David W.
Udry, Stephane
Marcy, Geoffrey W.
Isaacson, Howard
Howard, Andrew W.
Davies, Guy R.
Aguirre, Victor Silva
Kjeldsen, Hans
Bedding, Timothy R.
Lopez, Eric
Affer, Laura
Cosentino, Rosario
Figueira, Pedro
Fiorenzano, Aldo F. M.
Harutyunyan, Avet
Johnson, John Asher
Lopez-Morales, Mercedes
Lovis, Christophe
Mayor, Michel
Micela, Giusi
Molinari, Emilio
Motalebi, Fatemeh
Phillips, David F.
Piotto, Giampaolo
Queloz, Didier
Rice, Ken
Sasselov, Dimitar
Segransan, Damien
Sozzetti, Alessandro
Watson, Chris
Basu, Sarbani
Campante, Tiago L.
Christensen-Dalsgaard, Jorgen
Kawaler, Steven D.
Metcalfe, Travis S.
Handberg, Rasmus
Lund, Mikkel N.
Lundkvist, Mia S.
Huber, Daniel
Chaplin, William J.
TI THE KEPLER-454 SYSTEM: A SMALL, NOT-ROCKY INNER PLANET, A JOVIAN WORLD,
AND A DISTANT COMPANION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: composition; stars:
individual (KOI-273=KIC 3102384); asteroseismology; techniques: radial
velocities
ID MASS-RADIUS RELATIONSHIPS; STELLAR EVOLUTION CODE; FALSE-POSITIVE RATE;
100 EARTH MASSES; FUNDAMENTAL PROPERTIES; TERRESTRIAL PLANETS;
EXTRASOLAR PLANETS; SUPER-EARTHS; HOST STARS; HARPS-N
AB Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like star that hosts a transiting planet candidate in a 10.6 day orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i < 2.4 km s(-1). We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be 1.028(-0.03)(+0.04)M(circle dot), the radius to be 1.066 +/- 0.012 R-circle dot, and the age to be 5.25(-1.39)(+1.41) Gyr. We estimate the radius of the 10.6 day planet as 2.37 +/- 0.13 R-circle plus. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at the Keck Observatory, we measure the mass of this planet to be 6.8 +/- 1.4 M-circle plus. We also detect two additional nontransiting companions, a planet with a minimum mass of 4.46 +/- 0.12 M-J in a nearly circular 524 day orbit and a massive companion with a period >10 years and mass >12.1 M-J. The 12 exoplanets with radii <2.7 R-circle plus and precise mass measurements appear to fall into two populations, with those <1.6 R-circle plus following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 +/- 0.73 g cm(-3), Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.
C1 [Gettel, Sara; Charbonneau, David; Dressing, Courtney D.; Buchhave, Lars A.; Dumusque, Xavier; Vanderburg, Andrew; Latham, David W.; Johnson, John Asher; Lopez-Morales, Mercedes; Phillips, David F.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dressing, Courtney D.] CALTECH, Pasadena, CA USA.
[Dressing, Courtney D.] NASA, New York, NY USA.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Bonomo, Aldo S.; Sozzetti, Alessandro] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Malavolta, Luca; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy.
[Malavolta, Luca; Piotto, Giampaolo] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Pepe, Francesco; Udry, Stephane; Lovis, Christophe; Mayor, Michel; Motalebi, Fatemeh; Queloz, Didier; Segransan, Damien] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Cameron, Andrew Collier] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Davies, Guy R.; Campante, Tiago L.; Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Davies, Guy R.; Aguirre, Victor Silva; Kjeldsen, Hans; Bedding, Timothy R.; Campante, Tiago L.; Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Lund, Mikkel N.; Lundkvist, Mia S.; Huber, Daniel; Chaplin, William J.] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Bedding, Timothy R.; Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Lopez, Eric; Rice, Ken] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Affer, Laura; Micela, Giusi] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy.
[Cosentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet; Molinari, Emilio] Fdn Galileo Galilei, INAF, E-38712 Brena Baja, Spain.
[Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal.
[Molinari, Emilio] IASF Milano, INAF, I-20133 Milan, Italy.
[Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Watson, Chris] Queens Univ, Sch Math & Phys, Astrophys Res Ctr, Belfast, Antrim, North Ireland.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA.
RP Gettel, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sara.gettel@gmail.com
RI Rice, Ken/H-5084-2011; Figueira, Pedro/J-4916-2013;
OI Rice, Ken/0000-0002-6379-9185; Figueira, Pedro/0000-0001-8504-283X;
Malavolta, Luca/0000-0002-6492-2085; Cameron,
Andrew/0000-0002-8863-7828; Metcalfe, Travis/0000-0003-4034-0416;
Lundkvist, Mia Sloth/0000-0002-8661-2571; Handberg,
Rasmus/0000-0001-8725-4502; Lund, Mikkel Norup/0000-0001-9214-5642
FU NASA's Science Mission Directorate; Prodex Program of the Swiss Space
Office (SSO); Harvard University Origin of Life Initiative (HUOLI);
Scottish Universities Physics Alliance (SUPA); University of Geneva;
Smithsonian Astrophysical Observatory (SAO); Italian National
Astrophysical Institute (INAF); University of St. Andrews; Queen's
University Belfast; University of Edinburgh; European Union [313014];
John Templeton Foundation; National Aeronautics and Space Administration
[NNX15AC90G]; NASA [NNX13AE70G, NNX13AE91G]; Swiss National Science
Foundation (SNSF); National Science Foundation [1144152]; Fundacao para
a Ciencia e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013];
POPH/FSE (EC) by FEDER through the program "Programa Operacional de
Factores de Competitividade-COMPETE"; Fundacao para a Ciencia e a
Tecnologia (FCT) [IF/01037/2013CP1191/CT0001]; UK Science and Technology
Facilities Council (STFC); NSF [AST-1105930]; Danish National Research
Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations
with SONG and Kepler) - European Research Council [267864]; European
Community's Seventh Framework Programme [312844]; Kepler mission under
NASA Cooperation [NNX13AB58A]; W. M. Keck Foundation
FX The authors would like to thank the TNG observers who contributed to the
measurements reported here, including Walter Boschin, Massimo Cecconi,
Vania Lorenzi and Marco Pedani. We also thank Lauren Weiss for gathering
some of the HIRES data presented here. The authors wish to thank the
entire Kepler team, without whom these results would not be possible.
Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The HARPS-N project was funded by the Prodex Program of the
Swiss Space Office (SSO), the Harvard University Origin of Life
Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA),
the University of Geneva, the Smithsonian Astrophysical Observatory
(SAO), and the Italian National Astrophysical Institute (INAF),
University of St. Andrews, Queen's University Belfast and University of
Edinburgh. The research leading to these results has received funding
from the European Union Seventh Framework Programme (FP7/2007-2013)
under grant Agreement No. 313014 (ETAEARTH). This publication was made
possible by a grant from the John Templeton Foundation. The opinions
expressed in this publication are those of the authors and do not
necessarily reflect the views of the John Templeton Foundation. This
material is based upon work supported by the National Aeronautics and
Space Administration under grant No. NNX15AC90G issued through the
Exoplanets Research Program. C.D. is supported by a National Science
Foundation Graduate Research Fellowship. Work by C.D. was performed in
part under contract with the California Institute of Technology
(Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the
Sagan Fellowship Program executed by the NASA Exoplanet Science
Institute. X.D. would like to thank the Swiss National Science
Foundation (SNSF) for its support through an Early Postdoc Mobility
fellowship. A.V. is supported by the National Science Foundation
Graduate Research Fellowship, grant No. DGE 1144152. P. F. acknowledges
support by Fundacao para a Ciencia e a Tecnologia (FCT) through
Investigador FCT contracts of reference IF/01037/2013 and POPH/FSE (EC)
by FEDER funding through the program "Programa Operacional de Factores
de Competitividade-COMPETE". P.F. further acknowledges support from
Fundacao para a Ciencia e a Tecnologia (FCT) in the form of an
exploratory project of reference IF/01037/2013CP1191/CT0001. W.J.C.,
T.L.C. and G.R.D. acknowledge the support of the UK Science and
Technology Facilities Council (STFC). S.B. acknowledges partial support
from NSF grant AST-1105930 and NASA grant NNX13AE70G. T.S.M. was
supported by NASA grant NNX13AE91G. Computational time on Stampede at
the Texas Advanced Computing Center was provided through XSEDE
allocation TG-AST090107. Funding for the Stellar Astrophysics Centre is
provided by The Danish National Research Foundation (grant agreement
No.: DNRF106). The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement No.: 267864); and by the
European Community's Seventh Framework Programme (FP7/2007-2013) under
grant agreement No. 312844 (SPACEINN). Partial support was received from
the Kepler mission under NASA Cooperation Agreement NNX13AB58A to the
Smithsonian Astrophysical Observatory (PI:DWL).; Some of the data
presented herein were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics
and Space Administration. The Keck Observatory was made possible by the
generous financial support of the W. M. Keck Foundation. The spectra and
their products are made available at the NExSci Exoplanet Archive and
its CFOP website:. http://exoplanetarchive.ipac.caltech.edu. We thank
the many observers who contributed to the HIRES measurements reported
here, including Benjamin J. Fulton, Evan Sinukoff, and Lea Hirsch. We
gratefully acknowledge the efforts and dedication of the Keck
Observatory staff, especially Greg Doppmann, Scott Dahm, Hien Tran, and
Grant Hill for support of HIRES and Greg Wirth and Bob Goodrich for
support of remote observing. This research has made use of the NASA
Exoplanet Archive, which is operated by the California Institute of
Technology, under contract with the National Aeronautics and Space
Administration under the Exoplanet Exploration Program. Finally, the
authors wish to extend special thanks to those of Hawaiian ancestry on
whose sacred mountain of Mauna Kea we are privileged to be guests.
Without their generous hospitality, the Keck observations presented
herein would not have been possible.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 95
DI 10.3847/0004-637X/816/2/95
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500047
ER
PT J
AU Hung, CL
Hayward, CC
Smith, HA
Ashby, MLN
Lanz, L
Martinez-Galarza, JR
Sanders, DB
Zezas, A
AF Hung, Chao-Ling
Hayward, Christopher C.
Smith, Howard A.
Ashby, Matthew L. N.
Lanz, Lauranne
Martinez-Galarza, Juan R.
Sanders, D. B.
Zezas, Andreas
TI MERGER SIGNATURES IN THE DYNAMICS OF STAR-FORMING GAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: interactions; galaxies: kinematics and dynamics; galaxies:
structure
ID SMOOTHED PARTICLE HYDRODYNAMICS; ULTRALUMINOUS INFRARED GALAXIES;
ULTRA-DEEP-FIELD; H-ALPHA KINEMATICS; DIGITAL SKY SURVEY; LESS-THAN 1.5;
SIMILAR-TO 1; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES; INTERACTING
GALAXIES
AB The recent advent of integral field spectrographs and millimeter interferometers has revealed the internal dynamics of many hundreds of star-forming galaxies. Spatially resolved kinematics have been used to determine the dynamical status of star-forming galaxies with ambiguous morphologies, and constrain the importance of galaxy interactions during the assembly of galaxies. However, measuring the importance of interactions or galaxy merger rates requires knowledge of the systematics in kinematic diagnostics and the visible time with merger indicators. We analyze the dynamics of star-forming gas in a set of binary merger hydrodynamic simulations with stellar mass ratios of 1:1 and 1:4. We find that the evolution of kinematic asymmetries traced by star-forming gas mirrors morphological asymmetries derived from mock optical images, in which both merger indicators show the largest deviation from isolated disks during strong interaction phases. Based on a series of simulations with various initial disk orientations, orbital parameters, gas fractions, and mass ratios, we find that the merger signatures are visible for similar to 0.2-0.4 Gyr with kinematic merger indicators but can be approximately twice as long for equal-mass mergers of massive gas-rich disk galaxies designed to be analogs of z similar to 2-3 submillimeter galaxies. Merger signatures are most apparent after the second passage and before the black holes coalescence, but in some cases they persist up to several hundred Myr after coalescence. About 20%-60% of the simulated galaxies are not identified as mergers during the strong interaction phase, implying that galaxies undergoing violent merging process do not necessarily exhibit highly asymmetric kinematics in their star-forming gas. The lack of identifiable merger signatures in this population can lead to an underestimation of merger abundances in star-forming galaxies, and including them in samples of star-forming disks may bias the measurements of disk properties such as intrinsic velocity dispersion.
C1 [Hung, Chao-Ling; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Hung, Chao-Ling; Hayward, Christopher C.; Smith, Howard A.; Ashby, Matthew L. N.; Martinez-Galarza, Juan R.; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hung, Chao-Ling] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hayward, Christopher C.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Lanz, Lauranne] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece.
[Zezas, Andreas] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Crete, Greece.
RP Hung, CL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM chaoling.hung@gmail.com
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Hayward,
Christopher/0000-0003-4073-3236
FU NASA [NNX14AJ61G, NNX15AE56G]; Gordon and Betty Moore Foundation; FAS
Division of Science, Research Computing Group at Harvard University
FX C.-L.H., H.A.S., M.L.N.A., and J.R.M.-G. wish to acknowledge partial
funding support from NASA grants NNX14AJ61G and NNX15AE56G. C.C.H. is
grateful to the Gordon and Betty Moore Foundation for financial support.
The computations in this paper were run on the Odyssey cluster supported
by the FAS Division of Science, Research Computing Group at Harvard
University.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 99
DI 10.3847/0004-637X/816/2/99
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500051
ER
PT J
AU Joubert, T
Castro, D
Slane, P
Gelfand, J
AF Joubert, Timothy
Castro, Daniel
Slane, Patrick
Gelfand, Joseph
TI FERMI-LAT OBSERVATIONS OF SUPERNOVA REMNANT G5.7-0.1, BELIEVED TO BE
INTERACTING WITH MOLECULAR CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual
objects (G5.7-0.1); ISM: supernova remnants
ID GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; HIGH-ENERGY; 1720 MHZ; SHOCK
ACCELERATION; MASER EMISSION; INNER GALAXY; BROAD-BAND; OH MASERS; IC
443
AB This work reports on the detection of gamma-ray emission coincident with the supernova remnant (SNR) G5.7-0.1 using data collected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The SNR is believed to be interacting with molecular clouds, based on 1720 MHz hydroxyl (OH) maser emission observations in its direction. This interaction is expected to provide targets for the production of gamma-ray emission from pi(0)-decay. A gamma-ray source was observed in the direction of SNR G5.7-0.1, positioned near the bright gamma-ray source SNR W28. We model the emission from radio to gamma-ray energies using a one-zone model. Following consideration of both pi(0)-decay and leptonically dominated emission scenarios for the MeV-TeV source, we conclude that a considerable component of the gamma-ray emission must originate from the pi(0)-decay channel. Finally, constraints were placed on the reported ambiguity of the SNR distance through X-ray column density measurements made using XMM-Newton observations. We conclude G5.7-0.1 is a significant gamma-ray source positioned at a distance of similar to 3 kpc with luminosity in the 0.1-100 GeV range of L-gamma approximate to 7.4 x 10(34) erg s(-1).
C1 [Joubert, Timothy; Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Joubert, Timothy] Student Squadron, Laughlin AFB, TX 78843 USA.
[Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA.
[Gelfand, Joseph] NYU Abu Dhabi, Abu Dhabi, U Arab Emirates.
RP Joubert, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Gelfand, Joseph/0000-0003-4679-1058
FU National Aeronautics and Space Administration through the Smithsonian
Astrophysical Observatory [SV3-73016]; NASA [NAS8-03060]; National
Aeronautics Space Administration [NAS8-03060, NNX13AD56G]
FX D.C. acknowledges support for this work provided by the National
Aeronautics and Space Administration through the Smithsonian
Astrophysical Observatory contract SV3-73016 to MIT for Support of the
Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060. P. S. acknowledges support
from NASA Contract NAS8-03060. J.D.G. acknowledges support for analysis
of the XMM-Newton data through the National Aeronautics Space
Administration under grant NNX13AD56G. The authors would also like to
thank the helpful comments of the referee.
NR 53
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 63
DI 10.3847/0004-637X/816/2/63
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500015
ER
PT J
AU Maeda, K
Tajitsu, A
Kawabata, KS
Foley, RJ
Honda, S
Moritani, Y
Tanaka, M
Hashimoto, O
Ishigaki, M
Simon, JD
Phillips, MM
Yamanaka, M
Nogami, D
Arai, A
Aoki, W
Nomoto, K
Milisavljevic, D
Mazzali, PA
Soderberg, AM
Schramm, M
Sato, B
Harakawa, H
Morrell, N
Arimoto, N
AF Maeda, K.
Tajitsu, A.
Kawabata, K. S.
Foley, R. J.
Honda, S.
Moritani, Y.
Tanaka, M.
Hashimoto, O.
Ishigaki, M.
Simon, J. D.
Phillips, M. M.
Yamanaka, M.
Nogami, D.
Arai, A.
Aoki, W.
Nomoto, K.
Milisavljevic, D.
Mazzali, P. A.
Soderberg, A. M.
Schramm, M.
Sato, B.
Harakawa, H.
Morrell, N.
Arimoto, N.
TI SODIUM ABSORPTION SYSTEMS TOWARD SN Ia 2014J ORIGINATE ON INTERSTELLAR
SCALES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; dust, extinction; galaxies: individual (M82);
galaxies: ISM; supernovae: individual (SN 2014J)
ID HIGH-DISPERSION SPECTROGRAPH; HIGH-RESOLUTION SPECTRA;
HUBBLE-SPACE-TELESCOPE; SUPERNOVA 2014J; CIRCUMSTELLAR MATERIAL;
PROGENITOR SYSTEM; DIFFUSE BANDS; WHITE-DWARF; M82; EXTINCTION
AB Na I. D absorbing systems toward Type Ia supernovae (SNe Ia) have been intensively studied over the last decade with the aim of finding circumstellar material (CSM), which is an indirect probe of the progenitor system. However, it is difficult to deconvolve CSM components from non-variable, and often dominant, components created by interstellar material (ISM). We present a series of high-resolution spectra of SN. Ia. 2014J from before maximum brightness to greater than or similar to 250. days after maximum brightness. The late-time spectrum provides unique information for determining the origin of the Na I. D absorption systems. The deep late-time observation allows us to probe the environment around the SN at a large scale, extending to greater than or similar to 40 pc. We find that a spectrum of diffuse light in the vicinity, but not directly in the line of sight, of the SN has absorbing systems nearly identical to those obtained for the "pure" SN line of sight. Therefore, basically all Na I. D systems seen toward SN. 2014J must originate from foreground material that extends to at least similar to 40 pc in projection and none at the CSM scale. A fluctuation in the column densities at a scale of similar to 20 pc is also identified. After subtracting the diffuse, "background" spectrum, the late-time Na I. D profile along the SN line of sight is consistent with profiles near maximum brightness. The lack of variability on a similar to 1. year timescale is consistent with the ISM interpretation for the gas.
C1 [Maeda, K.; Nogami, D.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Maeda, K.; Moritani, Y.; Ishigaki, M.; Nomoto, K.; Schramm, M.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.
[Tajitsu, A.; Arimoto, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kawabata, K. S.; Moritani, Y.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Kawabata, K. S.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan.
[Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Honda, S.; Arai, A.] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
[Honda, S.; Hashimoto, O.] Gunma Astron Observ, Takayama, Gunma 3770702, Japan.
[Tanaka, M.; Aoki, W.; Harakawa, H.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Simon, J. D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Phillips, M. M.; Morrell, N.] Las Campanas Observ, Carnegie Observ, La Serena, Chile.
[Yamanaka, M.] Konan Univ, Dept Phys, Fac Sci & Engn, Kobe, Hyogo 6588501, Japan.
[Yamanaka, M.; Nogami, D.] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan.
[Milisavljevic, D.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Schramm, M.] Natl Inst Adv Ind Sci & Technol, Frequency Measurement Grp, Tsukuba, Ibaraki 3058563, Japan.
[Sato, B.; Harakawa, H.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
RP Maeda, K (reprint author), Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
EM keiichi.maeda@kusastro.kyoto-u.ac.jp
FU NASA [NAS. 5-26555]; World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan; Japan Society for the
Promotion of Science (JSPS) KAKENHI [26800100, 15H02075, 23224004,
26400222]; JSPS Open Partnership Bilateral Joint Research Project
between Japan and Chile; NSF [AST-1518052]; WPI Initiative, MEXT, Japan
FX The authors thank the staff at the Subaru Telescope, Okayama
observatory, and Gunma Astronomical observatory for their excellent
support of the observations, especially for the flexible arrangement and
the support of the ToO observations. We are especially grateful to H.
Izumiura and E. Kambe for their help in obtaining the ToO observations
with the OAO 1.88 m telescope. The authors thank M. Graham for kindly
providing the APF spectra of SN. 2014J and for stimulating discussion on
the K I absorbing systems. This paper uses data based on observations
made with the NASA/ESA Hubble Space Telescope, obtained from the data
archive at the Space Telescope Science Institute. STScI is operated by
the Association of Universities for Research in Astronomy, Inc. under
NASA contract NAS. 5-26555. The work by K. M. is partly supported by
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan. The work has been supported by Japan Society for the
Promotion of Science (JSPS) KAKENHI Grant 26800100 (K.M.), 15H02075,
15H00788 (M.T.), 23224004 and 26400222 (K.N.), and by JSPS Open
Partnership Bilateral Joint Research Project between Japan and Chile
(K.M.). R.J.F. gratefully acknowledges support from NSF grant
AST-1518052 and the Alfred P. Sloan Foundation. K.N. is supported by WPI
Initiative, MEXT, Japan.
NR 63
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 57
DI 10.3847/0004-637X/816/2/57
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500009
ER
PT J
AU Polito, V
Reep, JW
Reeves, KK
Simoes, PJA
Dudik, J
Del Zanna, G
Mason, HE
Golub, L
AF Polito, V.
Reep, J. W.
Reeves, K. K.
Simoes, P. J. A.
Dudik, J.
Del Zanna, G.
Mason, H. E.
Golub, L.
TI SIMULTANEOUS IRIS AND HINODE/EIS OBSERVATIONS AND MODELING OF THE 2014
OCTOBER 27 X2.0. CLASS FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: chromosphere; Sun: flares; techniques: spectroscopic
ID ULTRAVIOLET IMAGING SPECTROMETER; CORONAL DIAGNOSTIC SPECTROMETER; LOOP
RADIATIVE HYDRODYNAMICS; QUASI-SEPARATRIX LAYERS; X-RAY OBSERVATIONS;
SOLAR-FLARES; CHROMOSPHERIC EVAPORATION; IMPULSIVE PHASE; ATOMIC
DATABASE; ACTIVE-REGION
AB We present a study of the X2-class flare which occurred on 2014 October 27 and was observed with the Interface Region Imaging Spectrograph (IRIS) and the EUV Imaging Spectrometer (EIS) on board the Hinode satellite. Thanks to the high cadence and spatial resolution of the IRIS and EIS instruments, we are able to compare simultaneous observations of the Fe XXI 1354.08 angstrom. and Fe XXIII 263.77 angstrom high-temperature emission (greater than or similar to 10 MK) in the flare ribbon during the chromospheric evaporation phase. We find that IRIS observes completely blueshifted Fe XXI line profiles, up to 200 km s(-1) during the rise phase of the flare, indicating that the site of the plasma upflows is resolved by IRIS. In contrast, the Fe XXIII line is often asymmetric, which we interpret as being due to the lower spatial resolution of EIS. Temperature estimates from SDO/AIA and Hinode/XRT show that hot emission (log(T[K]) > 7.2) is first concentrated at the footpoints before filling the loops. Density-sensitive lines from IRIS and EIS give estimates of electron number density of greater than or similar to 10(12) cm(-3) in the transition region lines and 10(10) cm(-3) in the coronal lines during the impulsive phase. In order to compare the observational results against theoretical predictions, we have run a simulation of a flare loop undergoing heating using the HYDRAD 1D hydro code. We find that the simulated plasma parameters are close to the observed values that are obtained with IRIS, Hinode, and AIA. These results support an electron beam heating model rather than a purely thermal conduction model as the driving mechanism for this flare.
C1 [Polito, V.; Reep, J. W.; Del Zanna, G.; Mason, H. E.] Univ Cambridge, DAMTP, CMS, Wilberforce Rd, Cambridge CB3 0WA, England.
[Reep, J. W.] Naval Res Lab, Natl Res Council Postdoc Program, Washington, DC 20375 USA.
[Reeves, K. K.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
[Simoes, P. J. A.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Dudik, J.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
RP Polito, V (reprint author), Univ Cambridge, DAMTP, CMS, Wilberforce Rd, Cambridge CB3 0WA, England.
RI Dudik, Jaroslav/D-5876-2013;
OI Reep, Jeffrey/0000-0003-4739-1152; Reeves,
Katharine/0000-0002-6903-6832; Golub, Leon/0000-0001-9638-3082
FU Isaac Newton Studentship; Cambridge Trust; IRIS team at
Harvard-Smithsonian Centre for Astrophysics; RS Newton Alumni Programme;
NASA; STFC; Lockheed-Martin [8100002705]; European Community's Seventh
Framework Programme [606862]; Norwegian Space Center (NSC, Norway)
through an ESA PRODEX contract
FX V.P. acknowledges support from the Isaac Newton Studentship, the
Cambridge Trust, the IRIS team at Harvard-Smithsonian Centre for
Astrophysics and the RS Newton Alumni Programme. This research was
performed while J.W.R. held an NRC Research Associateship award at the
US Naval Research Laboratory with support from NASA, and previously a
PDRA at the University of Cambridge. H.E.M. and G.D.Z. acknowledge
support from the STFC and the RS Newton Alumni Programme. L.G. and K.R.
are supported by contract 8100002705 from Lockheed-Martin to SAO.
P.J.A.S. acknowledges support from the European Community's Seventh
Framework Programme (FP7/2007-2013) under grant agreement no. 606862
(F-CHROMA). J.D. acknowledges support from the RS Newton Alumni
Programme.r IRIS is a NASA small explorer mission developed and operated
by LMSAL with mission operations executed at NASA Ames Research center
and major contributions to downlink communications funded by the
Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract.
Hinode is a Japanese mission developed and launched by ISAS/JAXA, with
NAOJ as domestic partner and NASA and STFC (UK) as international
partners. It is operated by these agencies in cooperation with ESA and
NSC (Norway). AIA data are courtesy of NASA/SDO and the respective
science teams. CHIANTI is a collaborative project involving researchers
at the universities of Cambridge (UK), George Mason, and Michigan (USA).
NR 112
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 89
DI 10.3847/0004-637X/816/2/89
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500041
ER
PT J
AU Steffen, JH
Li, GJ
AF Steffen, Jason H.
Li, Gongjie
TI DYNAMICAL CONSIDERATIONS FOR LIFE IN MULTI-HABITABLE PLANETARY SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; celestial mechanics; meteorites, meteors, meteoroids;
planets and satellites: dynamical evolution and stability; planets and
satellites: terrestrial planets
ID LATE HEAVY BOMBARDMENT; OBLIQUITY VARIATIONS; ASTRONOMICAL THEORY;
CHAOTIC OBLIQUITY; EARTHS OBLIQUITY; CLIMATE CHANGES; MOONLESS EARTH;
SOLAR-SYSTEM; ICE AGES; MARS
AB Inspired by the close-proximity pair of planets in the Kepler-36 system, we consider two effects that may have important ramifications for the development of life in similar systems where a pair of planets may reside entirely in the habitable zone of the hosting star. Specifically, we run numerical simulations to determine whether strong, resonant (or non-resonant) planet-planet interactions can cause large variations in planet obliquity-thereby inducing large variations in climate. We also determine whether or not resonant interactions affect the rate of lithopanspermia between the planet pair-which could facilitate the growth and maintenance of life on both planets. We find that first-order resonances do not cause larger obliquity variations when compared with non-resonant cases. We also find that these resonant interactions are not a primary consideration in lithopanspermia. Lithopanspermia is enhanced significantly as the planet orbits come closer together-reaching nearly the same rate as ejected material falling back to the surface of the originating planet (assuming that the ejected material makes it out to the location of our initial conditions). Thus, in both cases our results indicate that close-proximity planet pairs in multi-habitable systems are conducive to life in the system.
C1 [Steffen, Jason H.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Steffen, Jason H.] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Li, Gongjie] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Steffen, JH (reprint author), Univ Nevada, Dept Phys & Astron, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA.
FU Lindheimer Fellowship at CIERA, Northwestern; NASA [NNX08AR04G]
FX We thank Konstantin Batygin for many useful discussions in the
preparation of this work. J.H.S. acknowledges support from the
Lindheimer Fellowship at CIERA, Northwestern, and from NASA under grant
NNX08AR04G, issued through the Kepler Participating Scientist Program.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 97
DI 10.3847/0004-637X/816/2/97
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500049
ER
PT J
AU Wang, T
Elbaz, D
Schreiber, C
Pannella, M
Shu, X
Willner, SP
Ashby, MLN
Huang, JS
Fontana, A
Dekel, A
Daddi, E
Ferguson, HC
Dunlop, J
Ciesla, L
Koekemoer, AM
Giavalisco, M
Boutsia, K
Finkelstein, S
Juneau, S
Barro, G
Koo, DC
Michalowski, MJ
Orellana, G
Lu, Y
Castellano, M
Bourne, N
Buitrago, F
Santini, P
Faber, SM
Hathi, N
Lucas, RA
Perez-Gonzalez, PG
AF Wang, T.
Elbaz, D.
Schreiber, C.
Pannella, M.
Shu, X.
Willner, S. P.
Ashby, M. L. N.
Huang, J. -S.
Fontana, A.
Dekel, A.
Daddi, E.
Ferguson, H. C.
Dunlop, J.
Ciesla, L.
Koekemoer, A. M.
Giavalisco, M.
Boutsia, K.
Finkelstein, S.
Juneau, S.
Barro, G.
Koo, D. C.
Michalowski, M. J.
Orellana, G.
Lu, Y.
Castellano, M.
Bourne, N.
Buitrago, F.
Santini, P.
Faber, S. M.
Hathi, N.
Lucas, R. A.
Perez-Gonzalez, P. G.
TI INFRARED COLOR SELECTION OF MASSIVE GALAXIES AT z > 3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
galaxies: structure
ID STAR-FORMING GALAXIES; SIMILAR-TO 4; SPECTRAL ENERGY-DISTRIBUTIONS;
EXTRAGALACTIC LEGACY SURVEY; REST-FRAME ULTRAVIOLET; SURVEY. SURVEY
DESIGN; EXTREMELY RED OBJECTS; QUASAR HOST GALAXIES; LYMAN BREAK
GALAXIES; GOODS-MUSIC SAMPLE
AB We introduce a new color selection technique to identify high-redshift, massive galaxies that are systematically missed by Lyman-break selection. The new selection is based on the H-160 (H) and Infrared Array Camera (IRAC) 4.5 mu m bands, specifically H - [4.5] > 2.25 mag. These galaxies, called "HIEROs," include two major populations that can be separated with an additional J - H color. The populations are massive and dusty starforming galaxies at z > 3 (JH - blue) and extremely dusty galaxies at z less than or similar to 3 (JH - red). The 350 arcmin(2) of the GOODS-North and GOODS-South fields with the deepest Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3) near-infrared and IRAC data contain as many as 285 HIEROs down to [4.5] < 24 mag. Inclusion of the most extreme HIEROs, not even detected in the H band, makes this selection particularly complete for the identification of massive high-redshift galaxies. We focus here primarily on JH - blue (z > 3) HIEROs, which have a median photometric redshift < z > similar to 4.4 and stellar mass M-* 10(10.6) M-circle dot and are much fainter in the rest-frame UV than similarly massive Lyman-break galaxies (LBGs). Their star formation rates (SFRs), derived from their stacked infrared spectral energy distributions (SEDs), reach similar to 240 M-circle dot yr(-1), leading to a specific SFR, sSFR equivalent to SFR/M-* similar to 4.2 Gyr(-1), suggesting that the sSFRs for massive galaxies continue to grow at z > 2 but at a lower growth rate than from z = 0 to z = 2. With a median half-light radius of 2 kpc, including similar to 20% as compact as quiescent (QS) galaxies at similar redshifts, JH - blue HIEROs represent perfect star-forming progenitors of the most massive (M-* greater than or similar to 10(11.2) M-circle dot) compact QS galaxies at z similar to 3 and have the right number density. HIEROs make up similar to 60% of all galaxies with M-* > 10(10.5) M-circle dot identified at z > 3 from their photometric redshifts. This is five times more than LBGs with nearly no overlap between the two populations. While HIEROs make up 15%-25% of the total SFR density at z similar to 4-5, they completely dominate the SFR density taking place in M-* 10(10.5) M-circle dot galaxies, and HIEROs are therefore crucial to understanding the very early phase of massive galaxy formation.
C1 [Wang, T.; Elbaz, D.; Schreiber, C.; Pannella, M.; Daddi, E.; Ciesla, L.; Juneau, S.] CEA DSM Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Shu, X.] Anhui Normal Univ, Dept Phys, Wuhu 241000, Anhui, Peoples R China.
[Willner, S. P.; Ashby, M. L. N.; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China.
[Huang, J. -S.] Chinese Acad Sci, China Chile Joint Ctr Astron, Camino El Observ, Santiago, Chile.
[Fontana, A.; Boutsia, K.; Castellano, M.; Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel.
[Ferguson, H. C.; Koekemoer, A. M.; Lucas, R. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Dunlop, J.; Michalowski, M. J.; Bourne, N.; Buitrago, F.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Finkelstein, S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Barro, G.; Koo, D. C.; Faber, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Orellana, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Lu, Y.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Hathi, N.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Perez-Gonzalez, P. G.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
RP Wang, T (reprint author), CEA DSM Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
EM tao.wang@cea.fr
RI Perez-Gonzalez, Pablo/J-2871-2016; Hathi, Nimish/J-7092-2014; Daddi,
Emanuele/D-1649-2012; Shu, Xinwen/D-7294-2017;
OI Perez-Gonzalez, Pablo/0000-0003-4528-5639; Hathi,
Nimish/0000-0001-6145-5090; Daddi, Emanuele/0000-0002-3331-9590; Shu,
Xinwen/0000-0002-7020-4290; Buitrago, Fernando/0000-0002-2861-9812;
Koekemoer, Anton/0000-0002-6610-2048
FU NASA [NAS5-26555]; European Union [312725]; National Natural Science
Foundation of China [11303014, 11133001, 11273015]; Spanish MINECO
[AYA2012-31277]
FX This work is based on observations taken by the CANDELS Multi-Cycle
Treasury Program and the 3D-HST Treasury Program with the NASA/ESA HST,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. This work is based in
part on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. Support for this work was
provided by NASA through an award issued by JPL/Caltech. The research
leading to these results has received funding from the European Union
Seventh Framework Program (FP7/2007-2013) under grant agreement No.
312725 (ASTRODEEP). T.W. acknowledges support for this work from the
National Natural Science Foundation of China under grants 11303014,
11133001, and 11273015. P.G. acknowledges support from Spanish MINECO
grant AYA2012-31277.
NR 110
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 84
DI 10.3847/0004-637X/816/2/84
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500036
ER
PT J
AU Wehrle, AE
Grupe, D
Jorstad, SG
Marscher, AP
Gurwell, M
Balokovic, M
Hovatta, T
Madejski, GM
Harrison, FH
Stern, D
AF Wehrle, Ann E.
Grupe, Dirk
Jorstad, Svetlana G.
Marscher, Alan P.
Gurwell, Mark
Balokovic, Mislav
Hovatta, Talvikki
Madejski, Grzegorz M.
Harrison, Fiona H.
Stern, Daniel
TI ERRATIC FLARING OF BL LAC IN 2012-2013: MULTIWAVELENGTH OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (BL Lacertae); galaxies: active;
galaxies: individual (BL Lacertae); galaxies: jets
ID ACTIVE GALACTIC NUCLEI; X-RAY TELESCOPE; SWIFT ULTRAVIOLET/OPTICAL
TELESCOPE; POLARIZATION VARIABILITY; SUPERLUMINAL MOTION; LACERTAE
OBJECTS; MAGNETIC-FIELD; 3C 454.3; JET; RADIO
AB BL Lac, the eponymous blazar, flared to historically high levels at millimeter, infrared, X-ray, and gamma-ray wavelengths in 2012. We present observations made with Herschel, Swift, NuSTAR, Fermi, the Submillimeter Array, CARMA, and the VLBA in 2012-2013, including three months with nearly daily sampling at several wavebands. We have also conducted an intensive campaign of 30 hr with every-orbit observations by Swift and NuSTAR, accompanied by Herschel, and Fermi observations. The source was highly variable at all bands. Time lags, correlations between bands, and the changing shapes of the spectral energy distributions can be explained by synchrotron radiation and inverse Compton emission from nonthermal seed photons originating from within the jet. The passage of four new superluminal very long baseline interferometry knots through the core and two stationary knots about 4 pc downstream accompanied the high flaring in 2012-2013. The seed photons for inverse Compton scattering may arise from the stationary knots and from a Mach disk near the core where relatively slow-moving plasma generates intense nonthermal radiation. The 95 spectral energy distributions obtained on consecutive days form the most densely sampled, broad wavelength coverage for any blazar. The observed spectral energy distributions and multi-waveband light curves are similar to simulated spectral energy distributions and light curves generated with a model in which turbulent plasma crosses a conical shock with a Mach disk.
C1 [Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA.
[Grupe, Dirk] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA.
[Grupe, Dirk] Swift Mission Operat Ctr, State Coll, PA 16801 USA.
[Jorstad, Svetlana G.; Marscher, Alan P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Jorstad, Svetlana G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Balokovic, Mislav; Hovatta, Talvikki; Harrison, Fiona H.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hovatta, Talvikki] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Madejski, Grzegorz M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wehrle, AE (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
EM awehrle@spacescience.org
RI Jorstad, Svetlana/H-6913-2013
OI Jorstad, Svetlana/0000-0001-9522-5453
FU NASA [NNX11AQ03G, NNX12AO79G, NNX13AP06G, NNX14AQ58G, NNX14AC59G,
NAS5-00136, NNG08FD60C]; Russian RFBR [15-02-00949]; St. Petersburg
University [6.38.335.2015]; Smithsonian Institution; Academia Sinica;
International Fulbright Science and Technology Award; NASA Headquarters
under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H];
National Aeronautics and Space Administration; Jenny and Antti Wihuri
foundation; Academy of Finland [267324]; Gordon and Betty Moore
Foundation; Kenneth T. and Eileen L. Norris Foundation; James S.
McDonnell Foundation; Associates of the California Institute of
Technology; University of Chicago; state of California; state of
Illinois; state of Maryland; National Science Foundation; CARMA partner
universities; Department of Energy in the United States; Commissariat
lEnergie Atomique; Centre National de la Recherche Scientifique/Institut
National de Physique Nuclaire et de Physique des Particules in France;
Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in
Italy; Ministry of Education, Culture, Sports, Science and Technology
(MEXT); High Energy Accelerator Research Organization (KEK); Japan
Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg
Foundation; Swedish Research Council; Swedish National Space Board in
Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National
dtudes Spatiales in France
FX A. Wehrle acknowledges Guest Investigator support from NASA via Herschel
RSA 1427799. The Boston University group acknowledges support by NASA
under Fermi Guest Investigator grants NNX11AQ03G, NNX12AO79G,
NNX13AP06G, and NNX14AQ58G, and Swift Guest Investigator grants
NNX14AC59G. S. G. Jorstad acknowledges support from Russian RFBR grant
15-02-00949 and St. Petersburg University research grant 6.38.335.2015.
The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica. The VLBA is an instrument of the National Radio
Astronomy Observatory. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. This research has made use of
the XRT Data Analysis Software (XRTDAS) developed under the
responsibility of the ASI Science Data Center (ASDC), Italy.; Swift at
PSU is supported by NASA contract NAS5-00136.; M. Balokovic acknowledges
support from the International Fulbright Science and Technology Award
and from NASA Headquarters under the NASA Earth and Space Science
Fellowship Program, grant NNX14AQ07H.; Part of this work was supported
under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR
mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the National
Aeronautics and Space Administration. We thank the NuSTAR Operations,
Software and Calibration teams for support with the execution and
analysis of these observations. This research has made use of the NuSTAR
Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(USA).; T. Hovatta acknowledges support from the Jenny and Antti Wihuri
foundation and Academy of Finland project number 267324. Support for
CARMA construction was derived from the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S.
McDonnell Foundation, the Associates of the California Institute of
Technology, the University of Chicago, the states of California,
Illinois, and Maryland, and the National Science Foundation. Ongoing
CARMA development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities.; The Fermi LAT Collaboration acknowledges generous ongoing
support from a number of agencies and institutes that have supported
both the development and the operation of the LAT as well as scientific
data analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat lEnergie Atomique and the Centre National de la Recherche
Scientifique/Institut National de Physique Nuclaire et de Physique des
Particules in France, the Agenzia Spaziale Italiana and the Istituto
Nazionale di Fisica Nucleare in Italy, the Ministry of Education,
Culture, Sports, Science and Technology (MEXT), High Energy Accelerator
Research Organization (KEK) and Japan Aerospace Exploration Agency
(JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National dtudes Spatiales in France.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2016
VL 816
IS 2
AR 53
DI 10.3847/0004-637X/816/2/53
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0ZV
UT WOS:000368238500005
ER
PT J
AU Farrior, CE
Bohlman, SA
Hubbell, S
Pacala, SW
AF Farrior, C. E.
Bohlman, S. A.
Hubbell, S.
Pacala, S. W.
TI Dominance of the suppressed: Power-law size structure in tropical
forests
SO SCIENCE
LA English
DT Article
ID GENERAL QUANTITATIVE THEORY; TREE SIZE; NEOTROPICAL FOREST; METABOLIC
ECOLOGY; TEMPERATE FOREST; GROWTH; DISTRIBUTIONS; DYNAMICS; MODEL;
DISTURBANCES
AB Tropical tree size distributions are remarkably consistent despite differences in the environments that support them. With data analysis and theory, we found a simple and biologically intuitive hypothesis to explain this property, which is the foundation of forest dynamics modeling and carbon storage estimates. After a disturbance, new individuals in the forest gap grow quickly in full sun until they begin to overtop one another. The two-dimensional space-filling of the growing crowns of the tallest individuals relegates a group of losing, slow-growing individuals to the understory. Those left in the understory follow a power-law size distribution, the scaling of which depends on only the crown area-to-diameter allometry exponent: a well-conserved value across tropical forests.
C1 [Farrior, C. E.] Natl Inst Math & Biol Synth, Knoxville, TN 37996 USA.
[Farrior, C. E.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA.
[Bohlman, S. A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA.
[Bohlman, S. A.; Hubbell, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Hubbell, S.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Pacala, S. W.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
RP Farrior, CE (reprint author), Natl Inst Math & Biol Synth, Knoxville, TN 37996 USA.
EM cfarrior@nimbios.org
FU Carbon Mitigation Initiative of Princeton University; National Institute
for Mathematical and Biological Synthesis (NSF, The University of
Tennessee, Knoxville) [DBI-1300426]
FX We thank J. Chave, H. C. Muller-Landau, and R. Chisholm for helpful
discussion and L. Comita for sharing data. We gratefully acknowledge the
support of the Carbon Mitigation Initiative of Princeton University and
the National Institute for Mathematical and Biological Synthesis (NSF
grant no. DBI-1300426, The University of Tennessee, Knoxville). The BCI
forest dynamics research project was founded by S. P. Hubbell and R. B.
Foster and is now managed by R. Condit, S. Lao, and R. Perez under the
Center for Tropical Forest Science and Smithsonian Tropical Research in
Panama. Numerous organizations have provided funding, principally in the
United States. NSF and hundreds of field workers have contributed. The
data are publicly available at
http://ctfs.arnarb.harvard.edu/webatlas/datasets/bci.
NR 27
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 8
PY 2016
VL 351
IS 6269
BP 155
EP 157
DI 10.1126/science.aad0592
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA4XQ
UT WOS:000367806500037
PM 26744402
ER
PT J
AU Kimura, M
Isogai, K
Kato, T
Ueda, Y
Nakahira, S
Shidatsu, M
Enoto, T
Hori, T
Nogami, D
Littlefield, C
Ishioka, R
Chen, YT
King, SK
Wen, CY
Wang, SY
Lehner, MJ
Schwamb, ME
Wang, JH
Zhang, ZW
Alcock, C
Axelrod, T
Bianco, FB
Byun, YI
Chen, WP
Cook, KH
Kim, DW
Lee, T
Marshall, SL
Pavlenko, EP
Antonyuk, OI
Antonyuk, KA
Pit, NV
Sosnovskij, AA
Babina, JV
Baklanov, AV
Pozanenko, AS
Mazaeva, ED
Schmalz, SE
Reva, IV
Belan, SP
Inasaridze, RY
Tungalag, N
Volnova, AA
Molotov, IE
de Miguel, E
Kasai, K
Stein, WL
Dubovsky, PA
Kiyota, S
Miller, I
Richmond, M
Goff, W
Andreev, MV
Takahashi, H
Kojiguchi, N
Sugiura, Y
Takeda, N
Yamada, E
Matsumoto, K
James, N
Pickard, RD
Tordai, T
Maeda, Y
Ruiz, J
Miyashita, A
Cook, LM
Imada, A
Uemura, M
AF Kimura, Mariko
Isogai, Keisuke
Kato, Taichi
Ueda, Yoshihiro
Nakahira, Satoshi
Shidatsu, Megumi
Enoto, Teruaki
Hori, Takafumi
Nogami, Daisaku
Littlefield, Colin
Ishioka, Ryoko
Chen, Ying-Tung
King, Sun-Kun
Wen, Chih-Yi
Wang, Shiang-Yu
Lehner, Matthew J.
Schwamb, Megan E.
Wang, Jen-Hung
Zhang, Zhi-Wei
Alcock, Charles
Axelrod, Tim
Bianco, Federica B.
Byun, Yong-Ik
Chen, Wen-Ping
Cook, Kem H.
Kim, Dae-Won
Lee, Typhoon
Marshall, Stuart L.
Pavlenko, Elena P.
Antonyuk, Oksana I.
Antonyuk, Kirill A.
Pit, Nikolai V.
Sosnovskij, Aleksei A.
Babina, Julia V.
Baklanov, Aleksei V.
Pozanenko, Alexei S.
Mazaeva, Elena D.
Schmalz, Sergei E.
Reva, Inna V.
Belan, Sergei P.
Inasaridze, Raguli Ya.
Tungalag, Namkhai
Volnova, Alina A.
Molotov, Igor E.
de Miguel, Enrique
Kasai, Kiyoshi
Stein, William L.
Dubovsky, Pavol A.
Kiyota, Seiichiro
Miller, Ian
Richmond, Michael
Goff, William
Andreev, Maksim V.
Takahashi, Hiromitsu
Kojiguchi, Naoto
Sugiura, Yuki
Takeda, Nao
Yamada, Eiji
Matsumoto, Katsura
James, Nick
Pickard, Roger D.
Tordai, Tamas
Maeda, Yutaka
Ruiz, Javier
Miyashita, Atsushi
Cook, Lewis M.
Imada, Akira
Uemura, Makoto
TI Repetitive patterns in rapid optical variations in the nearby black-hole
binary V404 Cygni
SO NATURE
LA English
DT Article
ID X-RAY BINARY; AMERICAN OCCULTATION SURVEY; TRANSIENT GS 2023+338;
DWARF-NOVA OUTBURSTS; GRS 1915+105; V4641 SAGITTARII; IGR J17091-3624;
LIGHT CURVES; GX 339-4; MASS DETERMINATIONS
AB How black holes accrete surrounding matter is a fundamental yet unsolved question in astrophysics. It is generally believed that matter is absorbed into black holes via accretion disks, the state of which depends primarily on the mass-accretion rate. When this rate approaches the critical rate (the Eddington limit), thermal instability is supposed to occur in the inner disk, causing repetitive patterns of large-amplitude X-ray variability (oscillations) on timescales of minutes to hours(1). In fact, such oscillations have been observed only in sources with a high mass-accretion rate, such as GRS 1915+105 (refs 2, 3). These large-amplitude, relatively slow timescale, phenomena are thought to have physical origins distinct from those of X-ray or optical variations with small amplitudes and fast timescales (less than about 10 seconds) often observed in other black-hole binaries-for example, XTE J1118+480 (ref. 4) and GX 339-4 (ref. 5). Here we report an extensive multi-colour optical photometric data set of V404 Cygni, an X-ray transient source(6) containing a black hole of nine solar masses(7) (and a companion star) at a distance of 2.4 kiloparsecs (ref. 8). Our data show that optical oscillations on timescales of 100 seconds to 2.5 hours can occur at mass-accretion rates more than ten times lower than previously thought(1). This suggests that the accretion rate is not the critical parameter for inducing inner-disk instabilities. Instead, we propose that a long orbital period is a key condition for these large-amplitude oscillations, because the outer part of the large disk in binaries with long orbital periods will have surface densities too low to maintain sustained mass accretion to the inner part of the disk. The lack of sustained accretion-not the actual rate-would then be the critical factor causing large-amplitude oscillations in long-period systems.
C1 [Kimura, Mariko; Isogai, Keisuke; Kato, Taichi; Ueda, Yoshihiro; Enoto, Teruaki; Hori, Takafumi; Nogami, Daisaku] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Nakahira, Satoshi] Japan Aerosp Explorat Agcy, Human Spaceflight Technol Directorate, JEM Mission Operat & Integrat Ctr, 2-1-1 Sengen, Tsukuba, Ibaraki 3058505, Japan.
[Shidatsu, Megumi] RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
[Enoto, Teruaki] Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan.
[Littlefield, Colin] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
[Ishioka, Ryoko; Chen, Ying-Tung; King, Sun-Kun; Wen, Chih-Yi; Wang, Shiang-Yu; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Jen-Hung; Zhang, Zhi-Wei; Cook, Kem H.; Lee, Typhoon] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan.
[Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19125 USA.
[Lehner, Matthew J.; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Axelrod, Tim] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bianco, Federica B.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[Byun, Yong-Ik] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
[Byun, Yong-Ik] Yonsei Univ, Univ Observ, Seoul 120749, South Korea.
[Chen, Wen-Ping] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
[Chen, Wen-Ping] Natl Cent Univ, Dept Phys, Chungli 32054, Taiwan.
[Kim, Dae-Won] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Marshall, Stuart L.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94309 USA.
[Pavlenko, Elena P.; Antonyuk, Oksana I.; Antonyuk, Kirill A.; Pit, Nikolai V.; Sosnovskij, Aleksei A.; Babina, Julia V.; Baklanov, Aleksei V.; Belan, Sergei P.] Crimean Astrophys Observ, Nauchnyi, Crimea, Ukraine.
[Pozanenko, Alexei S.; Mazaeva, Elena D.; Volnova, Alina A.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Pozanenko, Alexei S.] Natl Res Nucl Univ, MEPhI Moscow Engn Phys Inst, Moscow, Russia.
[Schmalz, Sergei E.] Leibniz Inst Astrophys, Potsdam, Germany.
[Reva, Inna V.] Fesenkov Astrophys Inst, Alma Ata, Kazakhstan.
[Inasaridze, Raguli Ya.] Ilia State Univ, Kharadze Abastumani Astrophys Observ, Tbilisi, Rep of Georgia.
[Tungalag, Namkhai] Mongolian Acad Sci, Inst Astron & Geophys, Ulaanbaatar 13343, Mongol Peo Rep.
[Molotov, Igor E.] Russian Acad Sci, Keldysh Inst Appl Math, Moscow, Russia.
[de Miguel, Enrique] Univ Huelva, Fac Ciencias Expt, Dept Fis Aplicada, Huelva 21071, Spain.
[de Miguel, Enrique] Observ CIECEM, Ctr Backyard Astrophys, Parque Dunar, Almonte 21760, Huelva, Spain.
[Kasai, Kiyoshi] Baselstr 133D, CH-4132 Muttenz, Switzerland.
[Stein, William L.] 6025 Calle Paraiso, Las Cruces, NM 88012 USA.
[Dubovsky, Pavol A.] Vihorlat Observ, Mierova 4, Humenne, Slovakia.
[Kiyota, Seiichiro] VSOLJ, 7-1 Kitahatsutomi, Chiba 2730126, Japan.
[Miller, Ian] Furzehill House, Swansea SA2 7LE, W Glam, Wales.
[Richmond, Michael] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
[Goff, William] AAVSO, 13508 Monitor Lane, Sutter Creek, CA 95685 USA.
[Andreev, Maksim V.] Russian Acad Sci, Inst Astron, Peak Terskol 361605, Kabardino Balka, Russia.
[Andreev, Maksim V.] Natl Acad Sci Ukraine, Int Ctr Astron Med & Ecol Res, 27 Akad Zabolotnoho St, UA-03680 Kiev, Ukraine.
[Takahashi, Hiromitsu] Hiroshima Univ, Sch Sci, Dept Phys Sci, 1-3-1 Kagamiyama, Hiroshima 7398526, Japan.
[Kojiguchi, Naoto; Sugiura, Yuki; Takeda, Nao; Yamada, Eiji; Matsumoto, Katsura] Osaka Kyoiku Univ, 4-698-1 Asahigaoka, Osaka 5828582, Japan.
[James, Nick] 1 Tavistock Rd, Chelmsford CM1 6JL, Essex, England.
[Pickard, Roger D.] BAA VSS, Burlington House, London W1J 0DU, England.
[Pickard, Roger D.] 3 Birches, Leominster HR6 9NG, Hereford, England.
[Tordai, Tamas] Hungarian Astron Assoc, Polaris Observ, Laborc Utca 2-C, H-1037 Budapest, Hungary.
[Maeda, Yutaka] 112-14 Kaminishiyama Machi, Nagasaki, Nagasaki 8500006, Japan.
[Ruiz, Javier] Observ Cantabria, Carretera Rocamundo Sin Numero, Valderredible, Cantabria, Spain.
[Ruiz, Javier] CSIC UC, Inst Fis Cantabria, Ave Los Castros Sin Numero, E-39005 Santander, Cantabria, Spain.
[Ruiz, Javier] Agrupac Astron Cantabra, Apartado 573, Santander 39080, Spain.
[Miyashita, Atsushi] Seikei High Sch, Seikei Meteorol Observ, Kichijoji Kitamachi 3-10-13, Tokyo 1808633, Japan.
[Cook, Lewis M.] Ctr Backyard Astrophys Concord, 1730 Helix Court, Concord, CA 94518 USA.
[Imada, Akira] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kitakazan Ohmine Cho, Kyoto 6078471, Japan.
[Imada, Akira] Kyoto Univ, Hida Observ, Yamashina Ku, Kitakazan Ohmine Cho, Kyoto 6078471, Japan.
[Uemura, Makoto] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Hiroshima 7398526, Japan.
RP Kimura, M (reprint author), Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
EM mkimura@kusastro.kyoto-u.ac.jp
RI de Miguel, Enrique/F-3734-2016; Shidatsu, Megumi/C-5742-2017;
OI de Miguel, Enrique/0000-0002-1381-8843; Lehner,
Matthew/0000-0003-4077-0985; Baklanov, Aleksei/0000-0001-7684-059X;
Cook, Lewis/0000-0003-3332-9649; Schwamb, Megan/0000-0003-4365-1455
FU thematic research program [AS-88-TP-A02]; Russian Science Foundation
[15-12-30016]; grant RUSTAVELI [FR/379/6-300/14]; Ministry of Education,
Culture, Sports, Science and Technology (MEXT) of Japan [25120007,
26400228]
FX We acknowledge the variable star observations from the AAVSO
International Database contributed by observers worldwide and used in
this research. We also thank the INTEGRAL groups for making the products
of the ToO data public online at the INTEGRAL Science Data Centre. Work
at ASIAA was supported in part by the thematic research program
AS-88-TP-A02. A.S.P., E.D.M. and A.A.V. are grateful to the Russian
Science Foundation (grant 15-12-30016) for support. R.Ya.I. is grateful
for partial support by the grant RUSTAVELI FR/379/6-300/14. We thank H.
Maehara, H. Akazawa, K. Hirosawa and J. Lluis for their optical
observations. This work was supported by the Grant-in-Aid "Initiative
for High-Dimensional Data-Driven Science through Deepening of Sparse
Modeling" from the Ministry of Education, Culture, Sports, Science and
Technology (MEXT) of Japan (25120007 TK and 26400228 YU).
NR 91
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 7
PY 2016
VL 529
IS 7584
BP 54
EP +
DI 10.1038/nature16452
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA6VY
UT WOS:000367944900024
PM 26738590
ER
PT J
AU Lyons, SK
Amatangelo, KL
Behrenstneyer, AK
Bercovici, A
Blois, JL
Davis, M
DiMichele, WA
Du, A
Eronen, JT
Faith, JT
Graves, GR
Jud, N
Labandeira, C
Looy, CM
McGill, B
Miller, JH
Patterson, D
Pineda-Munoz, S
Potts, R
Riddle, B
Terry, R
Toth, A
Ulrich, W
Villasenor, A
Wing, S
Anderson, H
Anderson, J
Waller, D
Gotelli, NJ
AF Lyons, S. Kathleen
Amatangelo, Kathryn L.
Behrenstneyer, Anna K.
Bercovici, Antoine
Blois, Jessica L.
Davis, Matt
DiMichele, William A.
Du, Andrew
Eronen, Jussi T.
Faith, J. Tyler
Graves, Gary R.
Jud, Nathan
Labandeira, Conrad
Looy, Cindy M.
McGill, Brian
Miller, Joshua H.
Patterson, David
Pineda-Munoz, Silvia
Potts, Richard
Riddle, Brett
Terry, Rebecca
Toth, Aniko
Ulrich, Werner
Villasenor, Amelia
Wing, Scott
Anderson, Heidi
Anderson, John
Waller, Donald
Gotelli, Nicholas J.
TI Holocene shifts in the assembly of plant and animal communities
implicate human impacts
SO NATURE
LA English
DT Article
ID NULL MODEL ANALYSIS; SPECIES COOCCURRENCE; ASSOCIATIONS; DISTRIBUTIONS;
BIODIVERSITY; QUATERNARY; EXTINCTIONS; DISPERSAL; DYNAMICS; PATTERNS
AB Understanding how ecological communities are organized and how they change through time is critical to predicting the effects of climate change(1). Recent work documenting the co-occurrence structure of modern communities found that most significant species pairs co-occur less frequently than would be expected by chance(2,3). However, little is known about how co-occurrence structure changes through time. Here we evaluate changes in plant and animal community organization over geological time by quantifying the co-occurrence structure of 359,896 unique taxon pairs in 80 assemblages spanning the past 300 million years. Co-occurrences of most taxon pairs were statistically random, but a significant fraction were spatially aggregated or segregated. Aggregated pairs dominated from the Carboniferous period (307 million years ago) to the early Holocene epoch (11,700 years before present), when there was a pronounced shift to more segregated pairs, a trend that continues in modern assemblages. The shift began during the Holocene and coincided with increasing human population size(4,5) and the spread of agriculture in North America(6,7). Before the shift, an average of 64% of significant pairs were aggregated; after the shift, the average dropped to 37%. The organization of modern and late Holocene plant and animal assemblages differs fundamentally from that of assemblages over the past 300 million years that predate the large-scale impacts of humans. Our results suggest that the rules governing the assembly of communities have recently been changed by human activity.
C1 [Lyons, S. Kathleen; Behrenstneyer, Anna K.; Bercovici, Antoine; Davis, Matt; DiMichele, William A.; Labandeira, Conrad; Toth, Aniko; Wing, Scott] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Amatangelo, Kathryn L.] SUNY Coll Brockport, Dept Environm Sci & Biol, Brockport, NY 14420 USA.
[Blois, Jessica L.] Univ Calif Merced, Sch Nat Sci, 5200 North Lake Rd, Merced, CA 95343 USA.
[Davis, Matt] Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA.
[Du, Andrew; Patterson, David; Villasenor, Amelia] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA.
[Eronen, Jussi T.] Univ Helsinki, Dept Geosci & Geog, POB 64, FIN-00014 Helsinki, Finland.
[Faith, J. Tyler] Univ Queensland, Sch Social Sci, Brisbane, Qld 4072, Australia.
[Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen, Denmark.
[Jud, Nathan] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA.
[Jud, Nathan] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Labandeira, Conrad] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Labandeira, Conrad] Capital Normal Univ, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China.
[Looy, Cindy M.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Looy, Cindy M.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA.
[McGill, Brian] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA.
[McGill, Brian] Univ Maine, Sustainabil Solut Initiat, Orono, ME 04469 USA.
[Miller, Joshua H.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA.
[Pineda-Munoz, Silvia] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia.
[Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Dept Anthropol, Washington, DC 20013 USA.
[Riddle, Brett] Univ Nevada, Sch Life Sci, Las Vegas, NV 89154 USA.
[Terry, Rebecca] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA.
[Ulrich, Werner] Nicholas Copernicus Univ, Chair Ecol & Biogeog, Lwowska 1, PL-87100 Torun, Poland.
[Anderson, Heidi; Anderson, John] Univ Witwatersrand, Evolutionary Studies Inst, Jorissen St, ZA-2001 Johannesburg, South Africa.
[Waller, Donald] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA.
[Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA.
RP Lyons, SK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
EM lyonss2@si.edu
RI Eronen, Jussi/B-7978-2013; publist, CMEC/C-3010-2012; McGill,
Brian/A-3476-2008; Blois, Jessica/G-5893-2011; publicationpage,
cmec/B-4405-2017;
OI Eronen, Jussi/0000-0002-0390-8044; McGill, Brian/0000-0002-0850-1913;
Blois, Jessica/0000-0003-4048-177X; Pineda-Munoz,
Silvia/0000-0003-0597-4456
FU National Museum of Natural History Program grant [NSF-DEB 1257625]
FX We thank G. Dietl for comments that improved the manuscript. Support for
this research was provided by a National Museum of Natural History
Program grant to the Evolution of Terrestrial Ecosystems Program (ETE)
and NSF-DEB 1257625. This is ETE publication 338.
NR 39
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 7
PY 2016
VL 529
IS 7584
BP 80
EP U183
DI 10.1038/nature16447
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA6VY
UT WOS:000367944900030
PM 26675730
ER
PT J
AU Crouse, DL
Philip, S
van Donkelaar, A
Martin, RV
Jessiman, B
Peters, PA
Weichenthal, S
Brook, JR
Hubbell, B
Burnett, RT
AF Crouse, Dan L.
Philip, Sajeev
van Donkelaar, Aaron
Martin, Randall V.
Jessiman, Barry
Peters, Paul A.
Weichenthal, Scott
Brook, Jeffrey R.
Hubbell, Bryan
Burnett, Richard T.
TI A New Method to Jointly Estimate the Mortality Risk of Long-Term
Exposure to Fine Particulate Matter and its Components
SO SCIENTIFIC REPORTS
LA English
DT Article
ID EXTENDED FOLLOW-UP; HARVARD 6 CITIES; AIR-POLLUTION;
CHEMICAL-CONSTITUENTS; COHORT; ASSOCIATIONS; HEALTH; PM2.5
AB Ambient fine particulate matter (PM2.5) is composed of a complex mixture of solids and liquids (smaller than 2.5 microns in aerodynamic diameter) derived from diverse sources (e.g., human activities, including fossil fuel combustion and industrial activities; and natural sources, including volcanic ash and pollens) that varies in space and time due to atmospheric chemistry, weather, and interactions between it and other pollutants in the atmosphere1. The composition of particulate matter, therefore, varies between and within regions of the world, countries, and urban and rural areas, and is influenced by such factors as climate, proximity to an ocean, agricultural activities, transportation activities, and kinds and quantities of point source emitters(2). The proximity to sources also affects the nature of the mixture of constituents composing PM2.5 (mixing state) with a greater propensity for external mixtures of particle types closer to sources, and more homogeneity among particle types as an air mass ages and the particles undergo a greater degree of atmospheric processing. The major components of PM2.5 typically consist of: sulphate; nitrate; ammonium; chloride/sea salt; carbon - described variously as elemental carbon, organic carbon, and black carbon; crustal material, including dust and minerals; and, biological materials and organic mass(2). The level of toxicity associated with PM2.5 is strongly affected by its mass and number concentrations, in addition to particle size, shape, chemical composition, and mixing state.
C1 [Crouse, Dan L.; Burnett, Richard T.] Hlth Canada, Environm Hlth Sci & Res Bur, Ottawa, ON K1A 0L2, Canada.
[Philip, Sajeev; van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jessiman, Barry] Hlth Canada, Air Qual Assessment Sect, Safe Environm Directorate, Ottawa, ON K1A 0L2, Canada.
[Peters, Paul A.] Univ New Brunswick, Dept Sociol, Fredericton, NB, Canada.
[Weichenthal, Scott] Hlth Canada, Safe Environm Directorate, Air Hlth Sci Div, Ottawa, ON K1A 0L2, Canada.
[Brook, Jeffrey R.] Environm Canada, Qual Res Div, Downsview, ON, Canada.
[Brook, Jeffrey R.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada.
[Hubbell, Bryan] US EPA, Off Air Qual Planning & Stand, Res Triangle Pk, NC 27711 USA.
RP Crouse, DL (reprint author), Hlth Canada, Environm Hlth Sci & Res Bur, Ottawa, ON K1A 0L2, Canada.
EM dan.crouse@unb.ca
RI Martin, Randall/C-1205-2014;
OI Martin, Randall/0000-0003-2632-8402; Peters, Paul/0000-0001-5225-2005;
Hubbell, Bryan/0000-0002-7963-3438
NR 30
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U1 6
U2 28
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD JAN 6
PY 2016
VL 6
AR 18916
DI 10.1038/srep18916
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA8YT
UT WOS:000368093600001
PM 26732864
ER
PT J
AU Mendes, CB
Matthews-Cascon, H
Norenburg, JL
AF Mendes, Cecili B.
Matthews-Cascon, Helena
Norenburg, Jon L.
TI New records of ribbon worms (Nemertea) from Ceara, Northeast Brazil
SO ZOOTAXA
LA English
DT Article
DE Occurrence; taxonomy; distribution
ID GREAT-BARRIER-REEF; PHYLUM NEMERTEA; PROSORHOCHMUS HOPLONEMERTEA; DELLE
CHIAJE; ANOPLA; HETERONEMERTEA; PHYLOGENY; ULTRASTRUCTURE;
CLASSIFICATION; MONOSTILIFERA
AB Of 45 species of nemerteans reported for the Brazilian coast, only two were recorded from Brazil's Northeast coast. Here we report seven new records for the state of Ceara, in Northeast Brazil: Tubulanus rhabdotus Correa, 1954, Carinomella cf. lactea Coe, 1905, Baseodiscus delineatus (Delle-Chiaje 1825), Cerebratulus cf. lineolatus Coe, 1905, Cerebratulus sp. 1, Cerebratulus sp. 2 and Lineidae sp. 1. Specimens were collected at the following beaches: Praia dos Dois Coqueiros, Praia do Pacheco, Pecem harbor, Praia da Pedra Rachada and Praia do Guajiru. T. rhabdotus is a new record for Northeast Brazil, Carinomella cf. lactea and Cerebratulus cf. lineolatus are new records for the South Atlantic Ocean and both genera are new records for Brazil.
C1 [Mendes, Cecili B.; Matthews-Cascon, Helena] Univ Fed Ceara, Lab Invertebrados Marinhos Ceara LIMCE, Dept Biol, Fortaleza, Ceara, Brazil.
[Mendes, Cecili B.; Matthews-Cascon, Helena] Univ Fed Ceara, Inst Ciencias Mar LABOMAR, Programa Posgrad Ciencias Marinhas Tropicais, Fortaleza, Ceara, Brazil.
[Norenburg, Jon L.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Mendes, CB (reprint author), Univ Fed Ceara, Lab Invertebrados Marinhos Ceara LIMCE, Dept Biol, Ave Mister Hull S-N,Campus Pici, Fortaleza, Ceara, Brazil.
EM cecilimendes@gmail.com
RI Mendes, Cecili/B-8886-2016
OI Mendes, Cecili/0000-0002-9041-1270
FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) of
the Ministry of Education of the Brazilian Government
FX We thank Robson de Jesus Mendes for assistance with histology, Paulo
Pachelle for helpful review of the manuscript and figures, Felipe A.C.
Monteiro for assistance with maps and the three anonymous reviewers. The
first author is grateful to Coordenacao de Aperfeicoamento de Pessoal de
Nivel Superior (CAPES) of the Ministry of Education of the Brazilian
Government, for providing financial support in the form of a MSc
scholarship fellowship.
NR 73
TC 0
Z9 0
U1 0
U2 5
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JAN 6
PY 2016
VL 4061
IS 2
BP 146
EP 156
PG 11
WC Zoology
SC Zoology
GA DA6BW
UT WOS:000367887700004
PM 27395488
ER
PT J
AU DiEuliis, D
Johnson, KR
Morse, SS
Schindel, DE
AF DiEuliis, Diane
Johnson, Kirk R.
Morse, Stephen S.
Schindel, David E.
TI OPINION Specimen collections should have a much bigger role in
infectious disease research and response
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Editorial Material
ID EMERGENCE; INFLUENZA; VIRUS
C1 [DiEuliis, Diane] US Dept HHS, Policy & Planning, Off Assistant Secretary Preparedness & Response, Washington, DC 20201 USA.
[Johnson, Kirk R.; Schindel, David E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Morse, Stephen S.] Columbia Univ, Mailman Sch Publ Hlth, Dept Epidemiol, New York, NY 10032 USA.
RP Schindel, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM schindeld@si.edu
OI Morse, Stephen/0000-0002-5434-5683
NR 18
TC 6
Z9 6
U1 0
U2 6
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 5
PY 2016
VL 113
IS 1
BP 4
EP 7
DI 10.1073/pnas.1522680112
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA0XH
UT WOS:000367520400019
PM 26733667
ER
PT J
AU Schnitzer, SA
van der Heijden, GMF
Powers, JS
AF Schnitzer, Stefan A.
van der Heijden, Geertje M. F.
Powers, Jennifer S.
TI REPLY TO VERBEECK AND KEARSLEY: Addressing the challenges of including
lianas in global vegetation models
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
ID REDUCE CARBON ACCUMULATION; TROPICAL FORESTS
C1 [Schnitzer, Stefan A.; van der Heijden, Geertje M. F.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA.
[Schnitzer, Stefan A.; van der Heijden, Geertje M. F.; Powers, Jennifer S.] Smithsonian Trop Res Inst, Panama City, Panama.
[van der Heijden, Geertje M. F.] Univ Nottingham, Sch Geog, Nottingham NG2 7RD, England.
[Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA.
[Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
RP Schnitzer, SA (reprint author), Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA.
EM s1@marquette.edu
NR 6
TC 1
Z9 1
U1 2
U2 5
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 5
PY 2016
VL 113
IS 1
BP E5
EP E6
DI 10.1073/pnas.1521823113
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA0XH
UT WOS:000367520400004
PM 26699499
ER
PT J
AU Duenas, LF
Tracey, DM
Crawford, AJ
Wilke, T
Alderslade, P
Sanchez, JA
AF Duenas, Luisa F.
Tracey, Dianne M.
Crawford, Andrew J.
Wilke, Thomas
Alderslade, Phil
Sanchez, Juan A.
TI The Antarctic Circumpolar Current as a diversification trigger for
deep-sea octocorals
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
DE Antarctic Circumpolar Current; Gene flow; Primnoid octocorals; Southern
Ocean; Deep-sea; Statistical phylogeography
ID DNA-SEQUENCE VARIATION; TRANSCRIBED SPACER-2 ITS2; MARINE BENTHIC
DIVERSITY; RNA SECONDARY STRUCTURES; SOUTHERN-OCEAN; NEW-ZEALAND;
GENETIC-VARIATION; DIVERGENCE TIMES; CNIDARIA OCTOCORALLIA; PHYLOGENETIC
ANALYSIS
AB Background: Antarctica is surrounded by the Antarctic Circumpolar Current (ACC), the largest and strongest current in the world. Despite its potential importance for shaping biogeographical patterns, the distribution and connectivity of deep-sea populations across the ACC remain poorly understood. In this study we conducted the first assessment of phylogeographical patterns in deep-sea octocorals in the South Pacific and Southern Ocean, specifically a group of closely related bottlebrush octocorals (Primnoidae: Tokoprymno and Thourella), as a test case to study the effect of the ACC on the population structure of brooding species. We assessed the degree to which the ACC constitutes a barrier to gene flow between northern and southern populations and whether the onset of diversification of these corals coincides with the origin of the ACC (Oligocene-Miocene boundary).
Results: Based on DNA sequences of two nuclear genes from 80 individuals and a combination of phylogeographic model-testing approaches we found a phylogenetic break corresponding to the spatial occurrence of the ACC. We also found significant genetic structure among our four regional populations. However, we uncovered shared haplotypes among certain population pairs, suggesting long-distance, asymmetrical migration. Our divergence time analyses indicated that the separation of amphi-ACC populations took place during the Middle Miocene around 12.6 million years ago, i.e., after the formation of the ACC.
Conclusion: We suggest that the ACC constitutes a semi-permeable barrier to these deep-sea octocorals capable of separating and structuring populations, while allowing short periods of gene flow. The fluctuations in latitudinal positioning of the ACC during the Miocene likely contributed to the diversification of these octocorals. Additionally, we provide evidence that the populations from each of our four sampling regions could actually constitute different species.
C1 [Duenas, Luisa F.; Crawford, Andrew J.; Sanchez, Juan A.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia.
[Duenas, Luisa F.; Wilke, Thomas; Sanchez, Juan A.] Univ Giessen, Dept Anim Ecol & Systemat, D-35390 Giessen, Germany.
[Tracey, Dianne M.] Natl Inst Water & Atmospher Res NIWA, Wellington, New Zealand.
[Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama.
[Alderslade, Phil] CSIRO Marine & Atmospher Res, Hobart, Tas 7001, Australia.
RP Duenas, LF (reprint author), Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia.
EM lf.duenas161@uniandes.edu.co
RI Wilke, Thomas/G-1517-2012;
OI Wilke, Thomas/0000-0001-8263-7758; Sanchez, Juan
Armando/0000-0001-7149-8369
FU Dr. David Bowden under NIWA's Ross Sea Climate & Ecosystem project
(Ministry of Business, Innovation and Employment contract) [CO1X1226];
New Zealand Ministry for Business, Innovation, and Employment; Fondo de
Investigacion de la Facultad de Ciencias at the Universidad de los Andes
in Bogota, Colombia; CEMarin
FX We would like to acknowledge Dr. Ben Sharp, Ministry for Primary
Industries (MPI) and New Zealand Scientific Committee representative to
the Commission for the Conservation of Antarctic Marine Living Resources
(CCAMLR) for approving the provision of the coral sample data; to MPI
and CCAMLR Observers for their at-sea collection of the corals. Several
NIWA experts have supported this research and we acknowledge their input
(Dr. Steve Parker, Dr. Sophie Mormede, Ms. Sadie Mills, Dr. Kareen
Schnabel). Dr. David Bowden provided funding for molecular analyses
under NIWA's Ross Sea Climate & Ecosystem project (Ministry of Business,
Innovation and Employment contract CO1X1226) and Dr. Aitana
Forcen-Vazquez (NIWA) produced Fig. 2a and provided useful comments on
the oceanic system for the study area. A portion of the material was
obtained during the New Zealand-Australian "MacRidge 2" research voyage
(TAN0803), that included the programme "Seamounts: their importance to
fisheries and marine ecosystems" funded by the New Zealand Ministry for
Business, Innovation, and Employment, and led by Drs. Ashely Rowden and
Malcolm Clark. We are also grateful to Dr. Kirrily Moore, invertebrate
collection manager, Tasmanian Museum and Art Gallery (TMAG) for the loan
of specimens. We are thankful for the insightful and constructive
comments from three anonymous reviewers. We would also like to
acknowledge the Fondo de Investigacion de la Facultad de Ciencias at the
Universidad de los Andes in Bogota, Colombia, which provided valuable
funds to LFD through the Proyecto Semilla program (Convocatoria 2014-2
para la Financiacion de Proyectos de Investigacion Categoria:
Estudiantes de Doctorado Candidatos). Additionally, we would like to
thank The Systematic Association and the Lerner Gray Memorial Fund that
also provided important support to LFD through The Systematics Research
Fund and The Lerner Gray Grant Award programs. Tavel support to LFD was
partially funded by CEMarin.
NR 108
TC 0
Z9 0
U1 3
U2 22
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD JAN 4
PY 2016
VL 16
AR 2
DI 10.1186/s12862-015-0574-z
PG 17
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA CZ9QA
UT WOS:000367430900002
PM 26727928
ER
PT J
AU Lin, XD
Shih, MJH
Labandeira, CC
Ren, D
AF Lin, Xiaodan
Shih, Matthew J. H.
Labandeira, Conrad C.
Ren, Dong
TI New data from the Middle Jurassic of China shed light on the phylogeny
and origin of the proboscis in the Mesopsychidae (Insecta: Mecoptera)
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
DE Evolutionary developmental model; Fossil insects; Inner Mongolia;
Mesozoic; Morphological characteristics; Scorpionfly
ID NORTHEASTERN CHINA; INNER-MONGOLIA; POLLINATION; SCORPIONFLIES;
SCARABAEOIDEA; COLEOPTERA; EVOLUTION; GYMNOSPERMS; LEPIDOPTERA; FAMILY
AB Background: The Mesopsychidae is an extinct family of Mecoptera, comprising eleven described genera from Upper Permian to Lower Cretaceous deposits. In 2009, several well-preserved mesopsychids with long proboscides were reported from the mid Mesozoic of Northeastern China, suggesting the presence of pollination mutualisms with gymnosperm plants and highlighting their elevated genus-level diversity. Since that time, additional mesopsychid taxa have been described. However, the phylogeny of genera within Mesopsychidae has not been studied formally, attributable to the limited number of well-preserved fossils.
Results: Here, we describe two new species, Lichnomesopsyche prochorista sp. nov. and Vitimopsyche pristina sp. nov. and revise the diagnosis of Lichnomesopsyche daohugouensis Ren, Labandeira and Shih, 2010, based on ten specimens from the latest Middle Jurassic Jiulongshan Formation of Inner Mongolia, China. After compiling data from these new fossil species and previously reported representative taxa, we conducted phylogenetic analyses and geometric morphometric studies that now shed light on the taxonomy and phylogeny of Mesopsychidae. We also evaluate the recurring origin of the siphonate proboscis in the Mecoptera and propose an evolutionary developmental model for its multiple origins.
Conclusions: Phylogenetic and geometric morphometric results confirm the establishment of two new species, each to Lichnomesopsyche and Vitimopsyche. Vitimopsyche pristina sp. nov. extends the existence of the genus Vitimopsyche Novokshonov and Sukacheva, 2001, from the mid Lower Cretaceous to the latest Middle Jurassic. Two methods of analyses indicate an affiliation of Mesopsyche dobrokhotovae Novokshonov, 1997 with Permopsyche Bashkuev, 2011. A phylogenetic analysis of the Mesopsychidae supports: 1), Mesopsychidae as a monophyletic group; 2), Mesopsyche as a paraphyletic group, to be revised pending future examination of additional material; and 3), the independent origin of the proboscis in the Pseudopolycentropodidae, its subsequent loss in earliest Mesopsychidae such as Epicharmesopsyche, its re-origination in the common ancestor (or perhaps independently) in the Vitimopsyche and Lichnomesopsyche clades of the Mesopsychidae. The third conclusion indicates that the proboscis originated four or five times within early Mecoptera, whose origin is explained by an evolutionary developmental model.
C1 [Lin, Xiaodan; Labandeira, Conrad C.; Ren, Dong] Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China.
[Shih, Matthew J. H.] Union Cty Magnet High Sch, Scotch Plains, NJ 07076 USA.
[Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA.
RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China.
EM rendong@mail.cnu.edu.cn
FU National Basic Research Program of China (973 Program) [2012CB821906];
National Natural Science Foundation of China [31230065, 41272006];
Beijing Municipal Commission of Education [KZ201310028033]; Program for
Changjiang Scholars and Innovative Research Team in University
[IRT13081]; Great Wall Scholar
FX We thank Dr. Yongjie Wang for his help and guidance for our use of the
phylogenetic and geometric morphometric software. We thank Drs. Taiping
Gao, Weiting Zhang, Qiang Yang and Chaofan Shi for their assistance in
improving the manuscript. We appreciate Longfeng Li, Sulin Liu, Xiao
Zhang, Yizi Cao and Chen Wang of Capital Normal University for their
valuable comments and fruitful suggestions. This research is supported
by the National Basic Research Program of China (973 Program)
(2012CB821906), the National Natural Science Foundation of China (No.
31230065, 41272006), Great Wall Scholar and KEY project of the Beijing
Municipal Commission of Education (KZ201310028033), Program for
Changjiang Scholars and Innovative Research Team in University
(IRT13081). This is contribution 313 of the Evolution of Terrestrial
Ecosystems consortium at the National Museum of Natural History, in
Washington, D.C.
NR 55
TC 3
Z9 3
U1 1
U2 10
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD JAN 4
PY 2016
VL 16
AR 1
DI 10.1186/s12862-015-0575-y
PG 22
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA CZ9QA
UT WOS:000367430900001
PM 26727998
ER
PT J
AU Brooker, RM
Brandl, SJ
Dixson, DL
AF Brooker, Rohan M.
Brandl, Simon J.
Dixson, Danielle L.
TI Cryptic effects of habitat declines: coral-associated fishes avoid
coral-seaweed interactions due to visual and chemical cues
SO SCIENTIFIC REPORTS
LA English
DT Article
ID GREAT-BARRIER-REEF; FEEDING BUTTERFLYFISHES CHAETODONTIDAE;
PHASE-SHIFTS; COMMUNITY STRUCTURE; KEYSTONE STRUCTURES; BIODIVERSITY;
MACROALGAE; DIVERSITY; CONSUMPTION; SPECIALIZATION
AB Seaweed-dominated coral reefs are becoming increasingly common as environmental conditions shift away from those required by corals and toward those ideal for rampant seaweed growth. How coral-associated organisms respond to seaweed will not only impact their fate following environmental change but potentially also the trajectories of the coral communities on which they rely. However, behavioral responses by coral-associated organisms to seaweeds are poorly understood. This study examined interactions between a guild of obligate and opportunistic coral-feeding butterflyfishes (Chaetodontidae) and scleractinian corals to determine whether fishes continue to interact with corals in contact with seaweed or if they are avoided. Under natural conditions, all species interacted almost exclusively with seaweed-free corals. In a controlled patch reef experiment, fishes avoided corals in physical contact with seaweed, irrespective of dietary preferences. When visual seaweed cues were removed, butterflyfish continued to avoid corals that had been in contact with the allelopathic Galaxaura filamentosa, suggesting that chemical cues produced by coral-seaweed interactions are repellent. These findings suggest that, due to deleterious visual and chemical cues produced by coralseaweed interactions, coral-associated organisms may struggle to locate resources as seaweed-free corals decline in abundance.
C1 [Brooker, Rohan M.; Dixson, Danielle L.] Univ Delaware, Sch Marine Sci & Policy, Lewes, DE 19958 USA.
[Brooker, Rohan M.; Dixson, Danielle L.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30318 USA.
[Brandl, Simon J.] Smithsonian Environm Res Ctr, Tennenbaum Marine Observ Network, Edgewater, MD 21037 USA.
[Brandl, Simon J.] James Cook Univ, Coll Trop & Marine Sci, Townsville, Qld 4811, Australia.
[Brandl, Simon J.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia.
RP Dixson, DL (reprint author), Univ Delaware, Sch Marine Sci & Policy, Lewes, DE 19958 USA.; Dixson, DL (reprint author), Georgia Inst Technol, Sch Biol, Atlanta, GA 30318 USA.
EM dixson@udel.edu
FU NSF [OCE-0929119]; Alfred P. Sloan Foundation
FX Support was provided by NSF grant OCE-0929119 and the Alfred P. Sloan
Foundation. We thank V. Bonito for assistance and the Fijian government
and the Korolevu-i-wai district elders for research permissions.
NR 60
TC 2
Z9 2
U1 4
U2 9
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD JAN 4
PY 2016
VL 6
AR 18842
DI 10.1038/srep18842
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH7SQ
UT WOS:000391973300001
PM 26725835
ER
PT J
AU Yang, LL
Huettmann, F
Brown, JL
Liu, SQ
Wang, WX
Yang, JY
Hu, DF
AF Yang, L. L.
Huettmann, F.
Brown, J. L.
Liu, S. Q.
Wang, W. X.
Yang, J. Y.
Hu, D. F.
TI Fecal glucocorticoid metabolite relates to social rank in Sichuan
snub-nosed monkeys
SO ITALIAN JOURNAL OF ZOOLOGY
LA English
DT Article
DE Sichuan snub-nosed monkey (Rhinopithecus roxellana); machine learning
and data mining; open access; dominance rank and stress; fecal
glucocorticoid metabolites (FGM)
ID NATIONAL NATURE-RESERVE; RHINOPITHECUS-ROXELLANA; CORTISOL-LEVELS;
CALLITHRIX-JACCHUS; QINLING MOUNTAINS; ADRENOCORTICAL FUNCTION; COMMON
MARMOSETS; DOMINANCE RANK; VERVET MONKEYS; LEMUR-CATTA
AB Studies suggest there is a connection between adrenal cortisol production and social rank in many non-human primates. Behavioral observations have confirmed that Sichuan snub-nosed monkeys (Rhinopithecus roxellana) have obvious social ranks. Thus, the goal of this study was to investigate whether there is a relationship between fecal glucocorticoid metabolite (FGM) concentrations as an indicator of social stress and dominance rank in Sichuan snub-nosed monkeys. Fecal samples were collected about every 5days for 1year from 10 Sichuan snub-nosed monkeys (> 7years old; n=5 males, 5 females), and analysed for FGM with a corticosterone radioimmunoassay using machine learning and open access data. Results showed that: (1) yearly mean FGM levels were negatively correlated with individual animal behavioral social rank in both males and females; (2) we divided the whole year into warm and cold seasons (seasonally) and breeding and nonbreeding seasons physiologically. Except for cold seasons, FGM levels have a negative correlation with behavioral social ranks in males and females; (3) female rank does not clearly relate to FGM levels; (4) social ranks of snub-nosed monkeys are more collaborative traits than aggressive ones. Our ?ndings have important implications for understanding the different physiological consequences of dominant and subordinate social status on Sichuan snub-nosed monkey societies, and it quantifies how physiological stress differs during seasons and phases, and by individuals.
C1 [Yang, L. L.; Liu, S. Q.; Wang, W. X.; Hu, D. F.] Beijing Forestry Univ, Coll Nat Conservat, Lab Noninvas Res Technol Endangered Wildlife, Beijing, Peoples R China.
[Huettmann, F.] Univ Alaska Fairbanks, Inst Arctic Biol, EWHALE Lab, Dept Biol & Wildlife, Fairbanks, AK USA.
[Brown, J. L.] Smithsonian Inst, Natl Zool Pk, Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA USA.
[Yang, J. Y.] Sichuan Snub Nosed Monkeys Res Inst Hu Bei Prov, Changsha, Hunan, Peoples R China.
RP Hu, DF (reprint author), Beijing Forestry Univ, Coll Nat Conservat, Lab Noninvas Res Technol Endangered Wildlife, Beijing, Peoples R China.
EM hudf@bjfu.edu.cn
FU Special Fund for Forestry Scientific Research in the Public Interest;
China's Ministry of Science and Technology [201004054]; EWHALE lab,
University of Alaska Fairbanks (UAF)
FX Fecal samples were collected by many Shennongjia Natural Reserve staff,
and population surveys were carried out by staff and students of Beijing
Forestry University. We appreciate Dr. Janine Brown's valuable advice
and work on the English writing. The managers of the Shenongjia Natural
Reserve allowed us to stay and do yearly records. Drs. Melissa Songer
and Zhang Dong kindly commented on and revised our earlier drafts.
Salford Systems Ltd. kindly allowed us to use their software for this
research. This study was funded by the Special Fund for Forestry
Scientific Research in the Public Interest, China's Ministry of Science
and Technology (No. 201004054) as well as the EWHALE lab, University of
Alaska Fairbanks (UAF).
NR 72
TC 0
Z9 0
U1 4
U2 7
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1125-0003
EI 1748-5851
J9 ITAL J ZOOL
JI Ital. J. Zoolog.
PD JAN 2
PY 2016
VL 83
IS 1
BP 15
EP 25
DI 10.1080/11250003.2015.1081707
PG 11
WC Zoology
SC Zoology
GA DF3NZ
UT WOS:000371252800003
ER
PT J
AU Suarez, C
Forasiepi, AM
Goin, FJ
Jaramillo, C
AF Suarez, Catalina
Forasiepi, Analia M.
Goin, Francisco J.
Jaramillo, Carlos
TI INSIGHTS INTO THE NEOTROPICS PRIOR TO THE GREAT AMERICAN BIOTIC
INTERCHANGE: NEW EVIDENCE OF MAMMALIAN PREDATORS FROM THE MIOCENE OF
NORTHERN COLOMBIA
SO JOURNAL OF VERTEBRATE PALEONTOLOGY
LA English
DT Article
ID LATITUDINAL DIVERSITY GRADIENT; MIDDLE MIOCENE; QUEBRADA-HONDA;
SOUTH-AMERICA; FALCON STATE; METATHERIA; TROPICS; BOLIVIA; VENEZUELA;
FAUNA
AB A new species of Sparassodonta (Mammalia, Metatheria), Lycopsis padillai, sp. nov., is described on the basis of a partial left maxilla with M1-M4 and fragments of lacrimal and jugal. The material comes from the early to early middle Miocene Castilletes Formation, La Guajira Peninsula, Colombia. This specimen represents the northernmost record of a fossil metatherian in South America and integrates a highly diverse vertebrate association, recently discovered in the north of Colombia. The La Guajira specimen is referred to the genus Lycopsis, as supported by the results of our phylogenetic analysis. This analysis also demonstrates that species of Lycopsis (L. torresi, L. longirostrus, L. viverensis, and L. padillai) constitute a monophyletic group and are placed as the basal taxon of Borhyaenoidea. Lycopsis padillai is a large-sized sparassodont with a body mass of about 22 kg. The presence of Lycopsis from La Guajira extends the geographical distribution of the genus to the entire South America, representing the sparassodont with the widest latitudinal distribution.
C1 [Suarez, Catalina; Forasiepi, Analia M.; Goin, Francisco J.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.
[Suarez, Catalina; Goin, Francisco J.] Museo La Plata, Div Paleontol Vertebrados, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina.
[Suarez, Catalina; Jaramillo, Carlos] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama.
[Forasiepi, Analia M.] Inst Argentino Nivol Glaciol & Ciencias Ambiental, Ave Ruiz Leal S-N, RA-5500 Mendoza, Mendoza Provinc, Argentina.
RP Suarez, C (reprint author), Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.; Suarez, C (reprint author), Museo La Plata, Div Paleontol Vertebrados, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina.; Suarez, C (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama.
EM catasuarezg@gmail.com; borhyaena@hotmail.com; fjgoin@fcnym.unlp.edu.ar;
JaramilloC@si.edu
FU Smithsonian Institution; National Geographic Society; Anders Foundation;
Gregory D. and Jennifer Walston Johnson; Universidad del Norte;
University of Zurich; National Science Foundation [EAR 0957679];
CONICET; Doris O. and Samuel P. Welles Research Fund of the UCMP;
Vertebrate Paleontology Endowment Fund at the FLMNH; Natural History
Museum of Los Angeles County
FX We thank E. Cadena who discovered the specimen described in this
document. The Smithsonian Institution, the National Geographic Society,
the Anders Foundation, Gregory D. and Jennifer Walston Johnson,
Universidad del Norte, the University of Zurich, and the National
Science Foundation (grant EAR 0957679) helped to support this work. We
thank A. Hendy, C. Montes, and students of the Universidad de Los Andes
for their contributions to the geology, stratigraphy, and
biostratigraphy of the area and help during the field activities; N.
Hoyos for GIS support; M. Reguero, S. Alvarez, and P. Holroyd for
permitting access to the collections under their care; M. Tomeo for
assistance with the illustrations; A. Scarano, F. Prevosti, N. Zimicz,
and T. Myers for their assistance with the body mass estimations; and F.
Vasconcellos for his suggestions. C. Suarez thanks CONICET for funding
her Ph.D. studies; the Doris O. and Samuel P. Welles Research Fund of
the UCMP, the Vertebrate Paleontology Endowment Fund at the FLMNH
(International Travel Grant to study the Vertebrate Paleontology
Collection), and K. Campbell (Natural History Museum of Los Angeles
County) and A. Stenger for financial support. J. Moreno, G. Ballen, F.
Moreno, M. C. Vallejo, J. Carrillo, C. Martinez, J. Luque, E. Cadena, J.
Carrillo, R. Sanchez, and C. Rosero kindly assisted during the field
trips in La Guajira. We thank the communities of Warpana, Patajau,
Aulechit, Nazareth, Wososopo, Sillamana, Paraguachon, La Flor de la
Guajira, and Ipapura; and the Colombian National Police (Castilletes
base) and the Colombian Army (La Flor de la Guajira and Cerro de la
Teta). We express special thanks to our drivers, Grillo, Lalo, and
Medardo. We acknowledge having used the Willi Hennig Society edition of
TNT. Editor M. Sanchez-Villagra and reviewers made constructive
suggestions for improvement of the manuscript.
NR 69
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U1 3
U2 8
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0272-4634
EI 1937-2809
J9 J VERTEBR PALEONTOL
JI J. Vertebr. Paleontol.
PD JAN 2
PY 2016
VL 36
IS 1
AR e1029581
DI 10.1080/02724634.2015.1029581
PG 10
WC Paleontology
SC Paleontology
GA DD6AW
UT WOS:000370007100005
ER
PT J
AU Briceno, RD
Eberhard, WG
Chinea-Cano, E
Wegrzynek, D
Rolo, TD
AF Briceno, R. D.
Eberhard, W. G.
Chinea-Cano, E.
Wegrzynek, D.
Rolo, T. dos Santos
TI Species-specific differences in the behavior of male tsetse fly
genitalia hidden in the female during copulation
SO ETHOLOGY ECOLOGY & EVOLUTION
LA English
DT Article
DE sexual selection; signals; genitalia; display traits; behavior genitalia
ID GLOSSINA-PALLIDIPES DIPTERA; SEXUAL SELECTION; MATING-BEHAVIOR;
MORPHOLOGY; EVOLUTION; FLIES; CHOICE; INSEMINATION; PHYLOGENY; MORSITANS
AB A long-standing question in morphological evolution is why male genitalia tend to diverge more rapidly than other structures. One possible explanation is that male genitalia are under sexual selection to function as internal courtship devices'. Males of closely related species may provide divergent stimulation using different genital morphologies and behaviors. Testing this hypothesis has been difficult, however, because the presumed genital courtship behavior is often hidden from view inside the female, and because studies of how the male's genitalia interact with those of the female are nearly always limited to a single species in a given group, thus restricting opportunities for comparison of closely related species. We present new morphological and behavioral data for portions of the male genitalia that are hidden in the female during copulation in five species in the tsetse fly genus Glossina using data from dissections of pairs frozen in copula, artificially stimulated males, and from copulating pairs viewed with a new X-ray technique that allows events inside the female to be recorded in real time. These data almost certainly give only an incomplete view of this complex, previously hidden world. But even so they clearly reveal that, as predicted by sexual selection theory, the male genitalia of Glossina flies perform dramatic, stereotyped, rhythmic movements deep within the female's reproductive tract and in inward folds of her external surface, and that many of these movements probably differ among closely related species. Most of the movements are not explicable as means by which the male anchors himself more securely to the female; all are likely to result in stimulation of the female. A female Glossina can be stimulated tactilely at a given moment during copulation at up to 8-10 or more different sites on her body.
C1 [Briceno, R. D.; Eberhard, W. G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica.
[Eberhard, W. G.] Louisiana State Univ, Smithsonian Trop Res Inst, Panama City, Panama.
[Eberhard, W. G.] Louisiana State Univ, Museum Nat Sci, Panama City, Panama.
[Eberhard, W. G.] Louisiana State Univ, Smithsonian Trop Res Inst, Baton Rouge, LA 70803 USA.
[Eberhard, W. G.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Chinea-Cano, E.; Wegrzynek, D.] IAEA, Instrumentat Unit, Agcy Labs Seibersdorf, A-1400 Vienna, Austria.
[Wegrzynek, D.] AGH Univ Sci & Technol, Fac Phys & Appl Comp Sci, PL-30059 Krakow, Poland.
[Rolo, T. dos Santos] Inst Technologyy KIT, Inst Photon Sci & Synchrotron Radiat, Karlsruhe, Germany.
RP Briceno, RD (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica.
EM rbriceno@biologia.ucr.ac.cr
RI dos Santos Rolo, Tomy/F-5511-2016
OI dos Santos Rolo, Tomy/0000-0002-9771-3511
FU IAEA; STRI (Smithsonian Tropical Research Institute Universidad);
Universidad de Costa Rica
FX We acknowledge the helpful assistance of Andrzej Markowicz from
International Atomic Energy Agency (IAEA) Seibersdorf Laboratories,
Christina Streli and Peter Wobrauschek from Atominstitut, Technical
University Vienna, Austria and the staff of the Forschungszentrum
Karlsruhe, in particular Alexander Rack, Timm Weitkamp, Patrik Vagovic
and Tilo Baumbach. This work could not have been completed without their
support and advice. We thank the IAEA for the use of flies and
facilities, Rudolf Boigner and Carmen Marin for help caring for flies,
D.M. Wood for advice concerning morphological homologies and Andrew
Parker, Marc Vreysen and Jorge Hendrichs for other kinds of help. The
IAEA, STRI (Smithsonian Tropical Research Institute Universidad) and the
Universidad de Costa Rica provided financial support.
NR 41
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U1 0
U2 12
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0394-9370
EI 1828-7131
J9 ETHOL ECOL EVOL
JI Ethol. Ecol. Evol.
PD JAN 2
PY 2016
VL 28
IS 1
BP 53
EP 76
DI 10.1080/03949370.2014.1002114
PG 24
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA CZ3KZ
UT WOS:000367004300005
ER
PT J
AU Vilas, LG
Guisande, C
Vari, RP
Pelayo-Villamil, P
Manjarres-Hernandez, A
Garcia-Rosello, E
Gonzalez-Dacosta, J
Heine, J
Perez-Costas, E
Granado-Lorencio, C
Palau-Ibars, A
Lobo, JM
AF Gonzalez Vilas, Luis
Guisande, Castor
Vari, Richard P.
Pelayo-Villamil, Patricia
Manjarres-Hernandez, Ana
Garcia-Rosello, Emilio
Gonzalez-Dacosta, Jacinto
Heine, Juergen
Perez-Costas, Elisa
Granado-Lorencio, Carlos
Palau-Ibars, Antoni
Lobo, Jorge M.
TI Geospatial data of freshwater habitats for macroecological studies: an
example with freshwater fishes
SO INTERNATIONAL JOURNAL OF GEOGRAPHICAL INFORMATION SCIENCE
LA English
DT Article
DE freshwater habitats; freshwater fishes; species richness; rarity
ID COMPARATIVE BIODIVERSITY; AGRICULTURAL LANDSCAPE; GLOBAL BIODIVERSITY;
SPECIES RICHNESS; SOFTWARE TOOL; PATTERNS; DIVERSITY; DATABASES;
CLIMATE; MODESTR
AB Global data sets are essential in macroecological studies. File formats of the few available data sets of freshwater ecosystems, however, are either incompatible with most macroecological software packages, incomplete, or of coarse spatial resolutions. We integrated more than 460 million geographical coordinates for freshwater habitats in the FRWater data set, partitioned into seven different habitats (lentic, wetlands, reservoirs, small rivers, large rivers, small ditches, large ditches, small channels, large channels, small drains and large drains) in ModestR (http://www.ipez.es/ModestR). A comprehensive collection of geospatial rasters was assembled, one for each of the seven freshwater habitats, with the area in km(2) occupied by each habitat presented in cells of 5arc-minute resolution. The utility of FRWater was evaluated using hierarchical partitioning via the identification of the contribution of the seven different freshwater habitats to both species richness and rarity. To this end, we used a data set of 836,123 geographical records of the 16,216 species of freshwater fishes recognized as valid by systematists at the end of 2014. Areas in North America and Europe are the most detailed in the FRWater data set, evidencing the higher quality of data sources in those regions. The number of geographical coordinates is much lower for Africa, Asia, Australia, and South America where many water bodies remain unmapped. In light of the variation in information quality at continental levels, we performed and present comparative analyses for Europe versus South America at local (5'x5' grid cells) and regional (5 degrees x5 degrees grid cells) scales. The relative contribution of small rivers to both species richness and rarity was highest under almost all analyses, followed by lentic habitats and large rivers. The areas of different habitats moreover explained a relatively high proportion of the observed variance in geographic rarity. Our findings corroborate previous findings that the greater contribution of small rivers to species richness is probably due to these habitats promoting geographical rarity. Hence, species richness is favored by the isolation resultant from, and the refuges associated with, small river basins and via the diversification processes promoted by such isolation.
C1 [Gonzalez Vilas, Luis; Guisande, Castor; Perez-Costas, Elisa] Univ Vigo, Fac Ciencias, Vigo 36310, Spain.
[Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Pelayo-Villamil, Patricia] Univ Antioquia, Grp Ictiol, Medellin, Colombia.
[Manjarres-Hernandez, Ana] Univ Nacl Colombia, Inst Amazon Invest IMANI, Leticia, Colombia.
[Garcia-Rosello, Emilio; Gonzalez-Dacosta, Jacinto; Heine, Juergen] Univ Vigo, Dept Informat, Vigo 36310, Spain.
[Granado-Lorencio, Carlos] Univ Seville, Fac Biol, Dept Biol Vegetal & Ecol, Seville, Spain.
[Palau-Ibars, Antoni] ENDESA, Direcc Medio Ambiente & Cambio Climat Espana & Po, I D I & Recursos Hidr, Biodiversidad, Lleida, Spain.
[Lobo, Jorge M.] CSIC, Museo Nacl Ciencias Nat, Dept Biogeog & Cambio Global, E-28006 Madrid, Spain.
RP Guisande, C (reprint author), Univ Vigo, Fac Ciencias, Vigo 36310, Spain.
EM castor@uvigo.es
FU ENDESA [110/02168]
FX This work was supported by the ENDESA [110/02168].
NR 48
TC 1
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U1 2
U2 23
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1365-8816
EI 1362-3087
J9 INT J GEOGR INF SCI
JI Int. J. Geogr. Inf. Sci.
PD JAN 2
PY 2016
VL 30
IS 1
SI SI
BP 126
EP 141
DI 10.1080/13658816.2015.1072629
PG 16
WC Computer Science, Information Systems; Geography; Geography, Physical;
Information Science & Library Science
SC Computer Science; Geography; Physical Geography; Information Science &
Library Science
GA CV3VY
UT WOS:000364195700010
ER
PT J
AU Dent, DH
Burslem, DFRP
AF Dent, Daisy H.
Burslem, David F. R. P.
TI Leaf traits of dipterocarp species with contrasting distributions across
a gradient of nutrient and light availability
SO PLANT ECOLOGY & DIVERSITY
LA English
DT Article
DE Foliar nutrient concentrations; leaf lifespan; leaf mass per area;
shade-tolerance; south-east Asia
ID TROPICAL RAIN-FOREST; TOLERANT TREE SEEDLINGS; PERFORMANCE TRADE-OFFS;
HABITAT ASSOCIATIONS; SHADE-TOLERANCE; LIFE-SPAN; RELATIVE IMPORTANCE;
COMMUNITY STRUCTURE; AMAZONIAN FORESTS; ROOT COMPETITION
AB Background: Tree species composition at the landscape scale is often tightly associated with underlying soil type in tropical forests. Changes in soil type may have effects on forest structure that drive changes in both light and soil resource availability, since light availability in the understorey tends to be lower in more fertile sites. Plant functional traits may determine species distributions across gradients of light and soil resource availability.
Aims: To test whether tree species with contrasting distributions exhibit leaf traits that reflect adaptation to the resources most limiting in their native environment.
Methods: We measured foliar nutrient concentrations, stomatal density, leaf delta C-13 values, leaf mass per area, and leaf lifespan for saplings of nine common dipterocarp species at Sepilok Forest Reserve, Malaysian Borneo, possessing varying associations to soil resource habitats.
Results: Species specialised in their adult distribution to nutrient-poor sandstone soils had traits indicative of a nutrient conservation strategy. Species specialised to more fertile alluvial soils had a wider spectrum of leaf N and P concentrations and LL, reflecting greater variance in strategies for resource acquisition and use among species in this habitat.
Conclusions: Understorey light regimes co-vary with soil type, and both light and soil resource availability influence leaf trait adaptations that may contribute to species-habitat associations.
C1 [Dent, Daisy H.] Univ Stirling, Biol & Environm Sci, Stirling, Scotland.
[Dent, Daisy H.] Smithsonian Trop Res Inst, Balboa, Panama.
[Burslem, David F. R. P.] Univ Aberdeen, Sch Biol Sci, Dept Plant & Soil Sci, Aberdeen, Scotland.
RP Dent, DH (reprint author), Univ Stirling, Biol & Environm Sci, Stirling, Scotland.; Dent, DH (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
EM daisy.h.dent@gmail.com
FU Natural Environment Research Council; British Ecological Society
FX This work was supported by the Natural Environment Research Council; the
British Ecological Society.
NR 92
TC 1
Z9 1
U1 0
U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1755-0874
EI 1755-1668
J9 PLANT ECOL DIVERS
JI Plant Ecol. Divers.
PY 2016
VL 9
IS 5-6
BP 521
EP 533
DI 10.1080/17550874.2016.1265018
PG 13
WC Plant Sciences
SC Plant Sciences
GA EP0CL
UT WOS:000397054300009
ER
PT J
AU Graves, GR
Dittmann, DL
Cardiff, SW
AF Graves, Gary R.
Dittmann, Donna L.
Cardiff, Steven W.
TI Diagnoses of hybrid hummingbirds (Aves: Trochilidae). 17. Documentation
of the intrageneric hybrid (Archilochus colubris X Archilochus
alexandri)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Archilochus alexandri; Archilochus colubris; Black-chinned Hummingbird;
hybridization; Ruby-throated Hummingbird
ID INTERGENERIC HYBRID; AVES TROCHILIDAE; SELASPHORUS-PLATYCERCUS;
SOUTHEASTERN ARIZONA; HYBRIDIZATION; SYSTEMATICS; MOUNTAINS; WOODSTAR;
ORIGIN; GOULD
AB Although the breeding ranges of Archilochus alexandri (Black-chinned Hummingbird) and Archilochus colubris (Ruby-throated Humming-bird) are narrowly parapatric in central Texas and central and southern Oklahoma, there have been few reports of hybridization in the literature and no well-documented hybrid specimens. Here we provide a comprehensive assessment of two male hybrids collected, respectively, in Grayson County, Texas, and East Baton Rouge Parish, Louisiana. As has been the pattern in other hummingbird hybrids, both specimens exhibit a blended mosaic of plumage characters of the parental species. Sequence for mitochondrial cytochrome c oxidase subunit 1 (CO1) for the hybrid specimen from East Baton Rouge Parish (LSU 182,831) confirms A. colubris as the female parent.
C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA.
[Graves, Gary R.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
[Dittmann, Donna L.; Cardiff, Steven W.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA.; Graves, GR (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
FU Smoketree Trust
FX We thank Gary Voelker (Texas A & M University) for lending the Grayson
County specimen, Faridah Dahlan for obtaining the COI sequence, and
several anonymous reviewers for comments on the manuscript. GRG was
supported by the Smoketree Trust.
NR 32
TC 0
Z9 0
U1 0
U2 0
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 1
EP 9
DI 10.2988/0006-324X-129.Q1.1
PG 9
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400001
ER
PT J
AU Munroe, TA
Kong, XY
AF Munroe, Thomas A.
Kong, Xiao-Yu
TI Resolving uncertainties regarding the nomenclature and status of the
Tongue Soles, Paraplagusia dollfusi Chabanaud, 1931 and "Cynoglossus
(Trulla) dollfusi (Chabanaud, 1937)'' (Teleostei: Pleuronectiformes:
Cynoglossidae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Nomenclature; Tonguefish; Red Sea; Flatfish; Cynoglossus; Paraplagusia;
Fringe-lip tongue soles; Cynoglossus cleopatridis
AB Considerable confusion surrounds the nomenclature and taxonomic status of the tongue sole, Paraplagusia dollfusi Chabanaud, 1931 (Cynoglossidae, Cynoglossinae), described from a single specimen captured in the Gulf of Suez, Red Sea, and Cynoglossus (Trulla) dollfusi Chabanaud, a name used by Gruvel and Chabanaud in 1937 for another specimen of tongue sole taken in the Suez Canal, Red Sea. Since publication, subsequent authors have considered there to be either one or two nominal species represented by these names, and authors have disagreed as to what genus (Paraplagusia, Cynoglossus, or both) nominal species associated with these names should be assigned. Both specimens have been reported as lost since at least the 1970s rendering it impossible to directly examine them to help resolve issues concerning their identities. We retrace historical literature involving these names and comment on reasons for the confusion experienced by previous authors. Our results, supported by irrefutable evidence gleaned from three different papers authored by Paul Chabanaud between 1931 and 1947, support the conclusion that only one valid nominal species is involved with these two names and the appropriate name for this taxon is Cynoglossus dollfusi (Chabanaud, 1931). Although never explicitly stated, nor indicated by use of appropriate punctuation in the descriptive account of the tongue sole specimen in the 1937 publication, we demonstrate that Gruvel and Chabanaud did not propose a new name when using the trinomial, Cynoglossus (Trulla) dollfusi, for this specimen. Rather, based on evidence uncovered in our investigation, as well as that appearing in a previously overlooked publication by Chabanaud in 1947, Cynoglossus (Trulla) dollfusi represents a new combination proposed by Gruvel and Chabanaud to reflect transfer of the nominal species, dollfusi, from Paraplagusia to Cynoglossus. Evidence is also provided to support the hypothesis, as has been suggested by previous authors, that appropriate generic assignment of Chabanaud's nominal species, dollfusi, is Cynoglossus, and not Paraplagusia.
C1 [Munroe, Thomas A.] NOAA, Natl Systemat Lab, NMFS, Natl Museum Nat Hist,NHB,Smithsonian Inst, POB 37012,MRC-153, Washington, DC 20013 USA.
[Kong, Xiao-Yu] Chinese Acad Sci, South China Sea Inst Oceanol, Key Lab Marine Bioresources Sustainable Utilizat, Guangzhou 510301, Guangdong, Peoples R China.
RP Munroe, TA (reprint author), NOAA, Natl Systemat Lab, NMFS, Natl Museum Nat Hist,NHB,Smithsonian Inst, POB 37012,MRC-153, Washington, DC 20013 USA.
EM munroet@si.edu; xykong@scsio.ac.cn
NR 26
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Z9 0
U1 0
U2 0
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 10
EP 23
DI 10.2988/0006-324X-129.Q1.10
PG 14
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400002
ER
PT J
AU Graves, GR
AF Graves, Gary R.
TI Head color and caruncles of sympatric Cathartes vultures (Aves:
Cathartidae) in Guyana and their possible function in intra-and
interspecific signaling
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE caruncles; Cathartes; Guyana; head color; intraspecific signal-ing
vulture
ID TURKEY VULTURES; MELAMBROTUS; SCAVENGERS; FOREST; FOOD
AB The naked heads of Cathartes vultures are widely believed to be adaptations for temperature regulation and to reduce plumage fouling during carrion feeding. Bright head color and the elaborate pattern of caruncles on the head and neck skin have a likely function in intra-and interspecific signaling. These integumentary characters have been difficult to study because of extensive postmortem color fading and shrinkage in museum specimens. Here I provide the first detailed description of head color and caruncles of the Greater Yellow-headed Vulture (C. melambrotus) from freshly collected specimens and provide comparative notes on sympatric populations of the Turkey Vulture (C. aura) and Lesser Yellow-headed Vulture (C. burrovianus) from Guyana.
C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA.
[Graves, Gary R.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA.; Graves, GR (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
EM gravesg@si.edu
NR 31
TC 1
Z9 1
U1 0
U2 0
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 66
EP 75
DI 10.2988/0006-324X-129.Q2.66
PG 10
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400007
ER
PT J
AU Woodman, N
Fisher, RD
AF Woodman, Neal
Fisher, Robert D.
TI Identification and distribution of the Olympic Shrew (Eulipotyphla:
Soricidae), Sorex rohweri Rausch et al., 2007 in Oregon and Washington,
based on USNM specimens
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE masked shrew; Pacific Northwest; Sorex vagrans; Soricomorpha; subspecies
AB Review of specimens of long-tailed shrews (Mammalia, Soricidae, Sorex) from the northwestern United States in the National Museum of Natural History (USNM), Washington, DC, has revealed the presence of the Olympic Shrew, Sorex rohweri Rausch et al., 2007, in the Coastal Range west of the Willamette Valley in Oregon. This determination nearly doubles the documented distribution for this species and increases the species diversity of soricids in Oregon to eleven. Sorex rohweri is relatively uncommon, but it occurs in a variety of forest successional stages and even clear cuts, as long as there is nearby forest and trees are allowed to regenerate. All USNM specimens from Washington formerly identified as S. cinereus streatori Merriam, 1895 are instead referable to the Olympic Shrew. The distribution of S. c. streatori is thereby restricted to the Pacific coasts of British Columbia north of the lower Frasier River and southcentral Alaska. Our study highlights the importance of taking and preserving high-quality voucher specimens in a collection where they are readily available for re-study.
C1 [Woodman, Neal; Fisher, Robert D.] USGS Patuxent Wildlife Res Ctr, Biol Survey Unit, Washington, DC 20013 USA.
[Woodman, Neal; Fisher, Robert D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Mammal Div, Washington, DC 20013 USA.
RP Woodman, N (reprint author), USGS Patuxent Wildlife Res Ctr, Biol Survey Unit, Washington, DC 20013 USA.; Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Mammal Div, Washington, DC 20013 USA.
EM woodmann@si.edu; fisherr@si.edu
NR 18
TC 0
Z9 0
U1 0
U2 0
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 84
EP 102
DI 10.2988/0006-324X-129.Q2.84
PG 19
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400009
ER
PT J
AU Phillips, AJ
Salas-Montiel, R
Oceguera-Figueroa, A
AF Phillips, Anna J.
Salas-Montiel, Ricardo
Oceguera-Figueroa, Alejandro
TI Distribution of the New England Medicinal Leech, Macrobdella sestertia
Whitman, 1886 and redeterminations of specimens of Macrobdella
(Annelida: Clitellata: Macrobdellidae) at the National Museum of Natural
History, Smithsonian Institution
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE copulatory glands; taxonomy; Hirudinea; geographic range; collections
AB The complete holdings of Macrobdella species at the Smithsonian's National Museum of Natural History were examined and the identity of 4 specimen lots were redetermined. One of these lots was redetermined as Macrobdella sestertia and represents the first report of this species from New Hampshire. Prior to this report, this species was only known from a few occurrences in eastern Massachusetts and Maine. This is also the first report of this species to be found in sympatry with Macrobdella decora, a more common congener with a widespread distribution.
C1 [Phillips, Anna J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 10th & Constitut Ave NW, Washington, DC 20560 USA.
[Salas-Montiel, Ricardo] Univ Nacl Autonoma Mexico, Inst Biol, Lab Helmintol, Posgrad Ciencias Biol, Tercer Circuito Sin Numero,Ciudad Univ,AP 70-153, Ciudad De Mexico 14510, Mexico.
[Oceguera-Figueroa, Alejandro] Univ Nacl Autonoma Mexico, Inst Biol, Lab Helmintol Eduardo Caballero & Caballero, Tercer Circuito Sin Numero,Ciudad Univ,AP 70-153, Ciudad De Mexico 14510, Mexico.
RP Phillips, AJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 10th & Constitut Ave NW, Washington, DC 20560 USA.
FU CONACYT; Posgrado en Ciencias Biologicas, UNAM
FX Thank you to William E. Moser and Karen Reed (both Department of
Invertebrate Zoology, NMNH) for visitor support during the visit of RSM
to the Museum Support Center, Smithsonian Institution and for access to
specimens in the collection. The visit of RSM to the NMNH was supported
by CONACYT and Posgrado en Ciencias Biologicas, UNAM. Thank you to Ted
R. Kahn for his expertise and assistance with the figures and to Joseph
O. Sexton ( University of Maryland) for his thoughtful advice about
ecoregions.
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PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 103
EP 113
DI 10.2988/0006-324X-129.Q2.103
PG 11
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400010
ER
PT J
AU Wang, ZM
Munroe, TA
Kong, XY
AF Wang, Zhong-ming
Munroe, Thomas A.
Kong, Xiao-yu
TI A new species of tongue sole (Pisces: Pleuronectiformes: Cynoglossidae:
Cynoglossus) from coastal waters of the South China Sea
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Flatfish; Tonguefish; Cynoglossid tongue sole
AB A new tongue sole, Cynoglossus nanhaiensis, described from 21 specimens (101.0-133.7 mm SL) collected in coastal waters of the South China Sea, is distinguished from congeners by the following combination of characters: 3 ocular-side lateral lines; no blind-side lateral lines; 2 ocular-side nostrils; 8 caudal-fin rays; 49-51 total vertebrae; 64-73 scales in the midlateral line; 11-12 scales in diagonal series between midlateral and dorsal lateral lines; 99-108 dorsal-fin rays; 77-82 anal-fin rays; pores of lateral-line scales tubular, with conspicuously black tips posteriorly; and with light-to medium-brown ocular-side background coloration overlain by numerous, small, irregular, dark blotches forming a series of narrow, interrupted, longitudinal stripes, with many specimens also featuring two large, brown spots on their caudal region. Among congeners, C. nanhaiensis is most similar to C. maccullochi Norman, 1926, described from specimens taken off Queensland, Australia, but differs in its ocular-side pigmentation (conspicuous longitudinal series of irregular blotches and caudal spots absent in C. maccullochi) and body depth. Features of C. nanhaiensis are also reminiscent of those reported for C. dollfusi (Chabanaud, 1931), a poorly-known nominal species from the Red Sea, and C. itinus (Snyder, 1909), a better-known species occurring in marine waters off Japan and Southeast Asia. Cynoglossus nanhaiensis differs from both species in having two (vs. one) ocular-side nostrils. Cynoglossus itinus also lacks the series of conspicuous, darkly-pigmented, interrupted, longitudinal stripes on the ocular side that are characteristic of C. nanhaiensis. Cynoglossus nanhaiensis is further distinguished from C. dollfusi in having only a single pelvic fin (vs. two in C. dollfusi). Cynoglossus nanhaiensis occurs in coastal waters of the South China Sea off southern China and Viet Nam.
C1 [Wang, Zhong-ming; Kong, Xiao-yu] Chinese Acad Sci, South China Sea Inst Oceanol, Key Lab Trop Marine Bioresources & Ecol, Guangzhou 510301, Guangdong, Peoples R China.
[Wang, Zhong-ming] Zhejiang Marine Fisheries Res Inst, Key Lab Sustainable Utilizat Technol Res Fishery, Zhoushan 316021, Peoples R China.
[Munroe, Thomas A.] NOAA, Natl Systemat Lab, NMFS, Smithsonian Inst,NHB, POB 37012,MRC-153, Washington, DC 20013 USA.
RP Kong, XY (reprint author), Chinese Acad Sci, South China Sea Inst Oceanol, Key Lab Trop Marine Bioresources & Ecol, Guangzhou 510301, Guangdong, Peoples R China.
EM zhmwangrch@163.com; munroet@si.edu; xykong@scsio.ac.cn
FU National Natural Science Foundation of China [31272273, 31471979,
31071890]
FX We thank students, H.-R. Luo and L. Gong, who helped with mailing
specimens and sending information regarding sexual maturity of specimens
examined in this study. S. Raredon (USNM) and L. Willis (NSL) provided
radiographs of specimens. L. Willis (NSL), H. Lopez-Fernandez and E.
Holm (ROM), and P.-L. Lin and M.-Y. Lee (ASIZP) assisted with specimens
and loans. We thank M.-Y. Lee for calling our attention to the large
specimen he collected in a fish market in Viet Nam. M. McGrouther (AMS),
J. Clayton (USNM) and K. Murphy (USNM) assisted with curation and
accessioning of specimens at their respective institutes. D. Gledhill
(CSIRO, Hobart, Australia) generously provided the photograph of
Cynoglossus maccullochi. R. Winterbottom (formerly of ROM) provided
additional information regarding the ROM specimen we examined. We thank
X.-L. Chen and two reviewers who provided helpful comments that improved
the manuscript. This study was supported by the National Natural Science
Foundation of China, grants 31272273, 31471979 and 31071890 (X.-Y. Kong,
principal investigator).
NR 42
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PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 129
EP 143
DI 10.2988/0006-324X-129.Q2.129
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400012
ER
PT J
AU Ernst, CH
Laemmerzahl, AF
Lovich, JE
AF Ernst, Carl H.
Laemmerzahl, Arndt F.
Lovich, Jeffrey E.
TI A morphological review of subspecies of the Asian box turtle, Cuora
amboinensis (Testudines, Geomydidae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Review
DE Asian box turtle; morphology; color patterns; subspecies
ID GENUS CUORA; MITOCHONDRIAL-DNA; EMYDIDAE; REPTILIA
AB The turtle Cuora amboinensis has an extensive distribution covering most of southern mainland Asia, Indonesia, and extending to the Philippine Islands. Unlike many species, C. amboinensis occurs on both sides of Wallace's Line separating Asian and Australian flora and fauna. Four subspecies are currently recognized; Cuora a. kamaroma (southern continental Asia, Java and the northern Philippines [introduced]), C. a. lineata (Kachin Province, Myanmar [Burma] and adjacent Yunnan Province, China), C. a. couro (Sumatra, Java, Sumbawa, and adjacent smaller Indonesian islands); and C. a. amboinensis (Moluccas, Sulawesi, Philippines). Five pattern and 33 morphological characters were examined for variation in 691 individuals from throughout the species' range. Our analyses suggest that only two presently recognized subspecies are valid: amboinensis and kamaroma. Neither couro nor lineata are supported by our analysis. We recommend that C. a. couro should be synonymized with the species C. amboinensis and C. a. lineata with the subspecies C. a. kamaroma.
C1 [Ernst, Carl H.] Smithsonian Inst, Div Amphibians & Reptiles, MRC 162,POB 37012, Washington, DC 20013 USA.
[Laemmerzahl, Arndt F.] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA.
[Lovich, Jeffrey E.] US Geol Survey, Southwest Biol Sci Ctr, 2255 North Gemini Dr, Flagstaff, AZ 86001 USA.
RP Ernst, CH (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, MRC 162,POB 37012, Washington, DC 20013 USA.
EM chernst@frontiernet.net
NR 32
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PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 144
EP 156
DI 10.2988/0006-324X-129.Q2.144
PG 13
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400013
ER
PT J
AU Cairns, SD
Zibrowius, H
AF Cairns, Stephen D.
Zibrowius, Helmut
TI Two new species of Flabellum (Scleractinia: Flabellidae) from the
Southwest Indian Ocean
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Flabellum; new species; Kerguelen; Heard Island; South Africa;
Flabellidae
AB Two new species of Flabellum are described from the southwest Indian Ocean, representing extremes of morphological variation within the genus. One of them, F. kerguelensis, is the first scleractinian coral reported from the Kerguelen Plateau. Flabellum now consists of 44 extant species, making it the fifth most species-rich genus in the order.
C1 [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Zibrowius, Helmut] Stn Marine Endoume, Rue Batterie des Lions, F-13007 Marseille, France.
RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
EM cairnss@si.edu
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PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 157
EP 163
DI 10.2988/0006-324X-129.Q2.157
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400014
ER
PT J
AU Lasley, RM
Ames, CL
Erdman, R
Parks, S
Collins, AG
AF Lasley, Robert M., Jr.
Ames, Cheryl Lewis
Erdman, Robert
Parks, Sheri
Collins, Allen G.
TI First record of the box jellyfish Tripedalia cystophora (Cnidaria:
Cubozoa: Tripedaliidae) in the Gulf of Mexico
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE box jellyfish; Tripedalia cystophora; Tripedaliidae; Cubozoa; Gulf of
Mexico; distribution
ID CARYBDEA-SIVICKISI CNIDARIA; CUBOMEDUSAE; SYNOPSIS; BEHAVIOR; MEDUSAE
AB Although observations of the box jellyfish Tripedalia cystophora have been widely documented since it was first recorded in Jamaica in 1897, to date there are no published reports of its occurrence in the Gulf of Mexico. Eighteen specimens of Tripedalia cystophora (Cubozoa: Tripedaliidae), 12 and 6, respectively, were collected from a mangrove waterway near Bonita Springs, Florida, in 2010 and a brackish canal in Englewood, Florida, in 2015. Additional records from Tampa Bay (2007-2015) and Everglades City (2015), Florida, were documented with photography. Within the past few years, new records of T. cystophora from other localities, including Hawai' i, northern Australia, and the east coast of Florida, have been reported. This study represents the first published report of the species from the Gulf of Mexico. Several other species of cubozoans have been reported from the Gulf region, but the presence of three pedalia at each corner of the swimming bell (12 tentacles total), its small size up to 13 mm, and the presence of sexually dimorphic gonads, markedly distinguishes it from other cubozoan taxa.
C1 [Lasley, Robert M., Jr.; Parks, Sheri] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL USA.
[Ames, Cheryl Lewis] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA.
[Erdman, Robert] Gulf Coast Univ, Dept Biol Sci, Ft Myers, FL USA.
[Collins, Allen G.] NOAA Fisheries, Natl Systemat Lab, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC USA.
RP Lasley, RM (reprint author), Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL USA.
EM Robert.Lasley@myfwc.com
NR 58
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PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 164
EP 172
DI 10.2988/0006-324X-129.Q2.164
PG 9
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400015
ER
PT J
AU Miller, AH
Zug, GR
AF Miller, Aryeh H.
Zug, George R.
TI Morphology and biology of the Asian Common Mockviper, Psammodynastes
pulverulentus (Boie, 1827) (Serpentes: Lamprophiidae): a focus on
Burmese populations
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Reptilia; Squamata; Myanmar; Burma; Thailand; morphometrics; scalation;
coloration; diet; reproduction; geographic variation; distribution
AB Psammodynastes pulverulentus occurs widely and is moderately abundant in the forests of Myanmar. The species shows morphological uniformity throughout its distribution from Kachin-Sagaing to Tanintharyi. Although there are no size differences among adult females (mean = 326, 253-436 mm SVL) and males (322, 222-471 mm SVL), a few morphological features are sexually dimorphic: adult females have shorter tails than adultmales (TailL/TotL means female female 17%, male male 20%) and relative head width and eye diameter are slightly larger in males. The number of ventral and subcaudal scales are only slightly different between females and males (median ventral, female female 158.5, male male 159; subcaudals, 54, 59.5, although significantly different). Our smaller Thai sample displayed the same pattern of variation in measurements and scalation as the Burmese sample. We developed a coding scheme for coloration and qualitatively demonstrate dimorphism in the Burmese sample; females are darker ventrally than males but females and males are the same dorsally. Other coloration traits are also dimorphic. In our Burmese sample, the number of adult males (n = 21) outnumbered females (18). Adult females were most abundant in the 251-300 mm SVL size class, males of near equal abundance in 201-250, 251-300, and 301-350 mm size classes. Relative to other Burmese snakes, P. pulverulentus ranked eighth in abundance, nearly equal number in frequency of occurrence with Dendrelaphis pictus. Our reproductive data do not clearly define reproductive periodicity and, based on large vitellogenic follicles, a likely clutch/litter size of 4 to 7. Although only 30% of our sample contained identifiable prey (frogs, lizards), most (67%) had digestive boluses in the lower half of the intestinal tract. Skinks were the dominant lizard prey and Limnonectes the dominant anurans. Uniformity or at least low differentiation between our Burmese and Thai samples and the results of Rasmussen (1975) advocate for the continued acceptance of the pan-Asian species concept for Psammodynastes pulverulentus.
C1 [Miller, Aryeh H.; Zug, George R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
EM amiller6@unca.edu; zugg@si.edu
FU Biodiversity program of the National Sciences Foundation [DEB-9971861,
DEB-0451832]; California Academy of Science (CAS); National Museum of
Natural History Smithsonian Institution (USNM)
FX Foremost, we wish to thank the Burmese members our Myanmar Herpetology
Survey (MHS) teams, all of which were staff of Myanmar's Nature and
Wildlife Conservation Division (NWCD), Forestry Department, for the
procurement of the Burmese sample of mockvipers. The success of the MHS
program resulted from the dedication and hard work of team members.
Surveys began in August 1997, although formally and most actively from
November 1999 through March 2010 with a hiatus in 2005 and 2006. Jens V.
Vindum, California Academy of Sciences, trained the team members in
herpetological field techniques and coordinated their field work (eight
to ten months each year) with the various directors of the NWCD. The
surveys were supported by the Biodiversity program of the National
Sciences Foundation (DEB-9971861, DEB-0451832), and assorted research
funds of the California Academy of Science (CAS) and the National Museum
of Natural History Smithsonian Institution (USNM). We thank the
preceding organizations and their administrative staffs for their
support and advocacy of this project. The authors acknowledge and thank
the collections management staffs of CAS and USNM for their ready
assistance in specimen and data access. JHM thanks the Chevy
Chase-Bethesda High School intern program and Ms. Stacy Farrar for
providing time during the regular school days and term to pursue this
research project. We also thank J. Block and J. Murphy for their careful
reviews of an early draft of the manuscript and three anonymous
reviewers for a final prepublication review.
NR 44
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PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PY 2016
VL 129
IS 1
BP 173
EP 194
DI 10.2988/0006-324X-129.Q2.173
PG 22
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA EM2XZ
UT WOS:000395180400016
ER
PT B
AU Shindell, M
AF Shindell, Matthew
BE Montgomery, GM
Largent, MA
TI GEOPHYSICS
SO COMPANION TO THE HISTORY OF AMERICAN SCIENCE
SE Wiley Blackwell Companions to American History
LA English
DT Article; Book Chapter
C1 [Shindell, Matthew] Smithsonian Inst, Natl Air & Space Museum, Solar Syst Explorat, Washington, DC 20560 USA.
[Shindell, Matthew] Harvard Univ, Cambridge, MA 02138 USA.
[Shindell, Matthew] Univ Southern Calif, Los Angeles, CA USA.
[Shindell, Matthew] Huntington Lib, San Marino, CA USA.
[Shindell, Matthew] Univ Calif San Diego, San Diego, CA 92103 USA.
[Shindell, Matthew] Chem Heritage Fdn, Philadelphia, PA USA.
RP Shindell, M (reprint author), Smithsonian Inst, Natl Air & Space Museum, Solar Syst Explorat, Washington, DC 20560 USA.
NR 0
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PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-119-07222-5; 978-1-4051-5625-7
J9 WILEY BLACK COMP AME
PY 2016
BP 120
EP 133
PG 14
WC History & Philosophy Of Science; History Of Social Sciences
SC History & Philosophy of Science; Social Sciences - Other Topics
GA BG0IN
UT WOS:000386252300011
ER
PT B
AU Henson, PM
AF Henson, Pamela M.
BE Montgomery, GM
Largent, MA
TI NATURAL HISTORY
SO COMPANION TO THE HISTORY OF AMERICAN SCIENCE
SE Wiley Blackwell Companions to American History
LA English
DT Article; Book Chapter
C1 [Henson, Pamela M.] Smithsonian Inst Archives, Inst Hist Div, Res & Documentat Hist Inst, Washington, DC 20560 USA.
RP Henson, PM (reprint author), Smithsonian Inst Archives, Inst Hist Div, Res & Documentat Hist Inst, Washington, DC 20560 USA.
NR 0
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PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, WEST SUSSEX, ENGLAND
BN 978-1-119-07222-5; 978-1-4051-5625-7
J9 WILEY BLACK COMP AME
PY 2016
BP 444
EP 455
PG 12
WC History & Philosophy Of Science; History Of Social Sciences
SC History & Philosophy of Science; Social Sciences - Other Topics
GA BG0IN
UT WOS:000386252300036
ER
PT J
AU Talamas, EJ
Masner, L
AF Talamas, Elijah J.
Masner, Lubomir
TI Revision of New World Helava Masner & Huggert (Platygastridae,
Sceliotrachelinae)
SO JOURNAL OF HYMENOPTERA RESEARCH
LA English
DT Article
DE Parasitoid; taxonomy; Platygastroidea
AB Nine new species of Helava are described: H. acutiventris sp. n., H. allomera sp. n., H. aureipes sp. n., H. carinata sp. n., H. microptera sp. n., H. pygmea sp. n., H. reducta sp. n., H. simplex sp. n., and H. samanthae sp. n., and Helava alticola Masner & Huggert is redescribed. New characters are presented to supplement the generic description of Masner and Huggert (1989) and the genus is diagnosed from similar genera in Sceliotrachelinae: Aphanomerus Dodd and Austromerus Masner & Huggert.
C1 [Talamas, Elijah J.] USNM, USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA.
[Masner, Lubomir] Agr & Agri Food Canada, KW Neatby Bldg, Ottawa, ON K1A 0C6, Canada.
RP Talamas, EJ (reprint author), USNM, USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA.
EM elijah.talamas@ars.usda.gov
FU Systematic Entomology Laboratory; National Institute of Food and
Agriculture-Specialty Crop Research Initiative (USDA-NIFA-SCRI)
[2011-51181-30937]
FX We thank Smithsonian interns Samantha Fitzsimmons Schoenberger and
Collin Schwantes for producing photographs and scanning electron
micrographs, respectively, and Norman Johnson (OSUC) for developing and
maintaining the Hymenoptera Online Database, Specimage, and vSysLab,
which underlie the cybertaxonomy conducted here. This work was made
possible by funding from the Systematic Entomology Laboratory and the
National Institute of Food and Agriculture-Specialty Crop Research
Initiative (USDA-NIFA-SCRI) # 2011-51181-30937. The USDA does not
endorse any commercial product mentioned in this research. USDA is an
equal opportunity provider and employer.
NR 4
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PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1070-9428
EI 1314-2607
J9 J HYMENOPT RES
JI J. Hymenopt. Res.
PY 2016
VL 53
BP 1
EP 24
DI 10.3897/jhr.53.10217
PG 24
WC Entomology
SC Entomology
GA EL2KC
UT WOS:000394447600001
ER
PT J
AU Lue, CH
Driskell, AC
Leips, J
Buffington, ML
AF Lue, Chia-Hua
Driskell, Amy C.
Leips, Jeff
Buffington, Matthew L.
TI Review of the genus Leptopilina (Hymenoptera, Cynipoidea, Figitidae,
Eucoilinae) from the Eastern United States, including three newly
described species
SO JOURNAL OF HYMENOPTERA RESEARCH
LA English
DT Review
DE Parasitoid wasps; Drosophila; Nearctic Region; geographic distribution;
DNA barcoding
ID DROSOPHILA; PARASITOIDS; PHYLOGENY; DIVERSITY; EVOLUTION; REVISION;
TAXONOMY; GENERA
AB The genus Leptopilina has historically been a poorly understood group. However, some species of Leptopilina are among the best-known model organisms for studying host-parasitoid interactions. As there is no identification system for Leptopilina in any part of the United States, we review species that were collected throughout their range in Eastern North America and those commonly used in laboratories. We provide a key for seven species, L. boulardi, L. heterotoma, L. clavipes, L. victoriae, L. decemflagella sp. n., L. maia sp. n. and L. leipsi sp. n., the last three of which are newly described here. This study is the first of its kind for Leptopilina species in North America, as our review and key were developed by examining a large number of specimens collected across broad chronological and geographic scales. This allowed us to account for the phenotypic variation within species, and helped us discover diagnostic characters. The geographic distribution and taxonomic information from this review provides a solid foundation for future research on Leptopilina.
C1 [Lue, Chia-Hua; Leips, Jeff] Univ Maryland Baltimore Cty, Dept Biol Sci, 1000 Hilltop Circle, Baltimore, MD 21042 USA.
[Driskell, Amy C.] Natl Museum Nat Hist, Labs Analyt Biol, Smithsonian Inst, 10th & Constitut Ave NW, Washington, DC 20560 USA.
[Lue, Chia-Hua; Buffington, Matthew L.] Natl Museum Nat Hist, Systemat Entomol Lab, USDA ARS, Smithsonian Inst, 10th & Constitut Ave NW, Washington, DC 20560 USA.
RP Lue, CH (reprint author), Univ Maryland Baltimore Cty, Dept Biol Sci, 1000 Hilltop Circle, Baltimore, MD 21042 USA.; Lue, CH (reprint author), Natl Museum Nat Hist, Systemat Entomol Lab, USDA ARS, Smithsonian Inst, 10th & Constitut Ave NW, Washington, DC 20560 USA.
EM chia3@umbc.edu
FU USNM; UMBC (University of Maryland Baltimore County)
FX We gratefully acknowledge the support of the owners of One Straw Farm,
Weber Farm, Robert Is Here, Fruit and Spice Park, Orchard Pond Organic
Farm and Musser Fruit Research Farm for allowing us to sample on their
property. We thank Dr. Todd Schlenke, Dr. Masahito Kimura and Dr.
Mattias Forshage for providing personal parasitoid collections for
reference samples. We thank Dr. Kenneth MacDonald for his assistance
with molecular work. We thank Dr. Norm Johnson and Sara Hemly (OSU) for
assistance using vSyslab. We also thank Dr. Elijah Talamas for advise
with image processing in the Hymenoptera Imaging Suite at the USNM and
Mr. Tim Ford in UMBC. All the molecular laboratory work was conducted in
and with the support of the L.A.B. facilities of the National Museum of
Natural History. This study has been supported by a USNM graduate
student fellowship to CHL, and UMBC (University of Maryland Baltimore
County). Drs. Jose-Luis Nieves-Aldrey, George Melika, Mattias Forshage
and Matthew Yoder reviewed and helped greatly improve this paper.
Mention of trade names or commercial products in this publication is
solely for the purpose of providing specific information does not imply
recommendation or endorsement by the USDA. USDA is an equal opportunity
provider and employer.
NR 33
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PU PENSOFT PUBL
PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1070-9428
EI 1314-2607
J9 J HYMENOPT RES
JI J. Hymenopt. Res.
PY 2016
VL 53
BP 35
EP 76
DI 10.3897/jhr.53.10369
PG 42
WC Entomology
SC Entomology
GA EL2KC
UT WOS:000394447600003
ER
PT J
AU Smith, DR
AF Smith, David R.
TI Two unusual new species of Aulacus Jurine (Hymenoptera,Aulacidae) from
South America
SO JOURNAL OF HYMENOPTERA RESEARCH
LA English
DT Article
DE parasitoids; South America
ID AULACIDAE HYMENOPTERA
AB Aulacus flavus Smith, sp. n. from Brazil and Aulacus subflavus Smith, sp. n. from Brazil, French Guiana, and Guyana are described. These two species are separated from other Aulacus by the enlarged genae, flat mesoscutum, enlarged pronotum, and presence of small tubercles on the mesoprescutum, axillae, and mesoscutellum.
C1 [Smith, David R.] Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, POB 37012,MRC 168, Washington, DC 20013 USA.
RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, POB 37012,MRC 168, Washington, DC 20013 USA.
EM sawfly2@aol.com
NR 8
TC 0
Z9 0
U1 0
U2 0
PU PENSOFT PUBL
PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1070-9428
EI 1314-2607
J9 J HYMENOPT RES
JI J. Hymenopt. Res.
PY 2016
VL 53
BP 163
EP 170
DI 10.3897/jhr.53.9902
PG 8
WC Entomology
SC Entomology
GA EL2KC
UT WOS:000394447600005
ER
PT J
AU Gibbons, S
AF Gibbons, Sarah
TI "Our Furniture Family": Frasier's Luxury Problems
SO LUXURY-HISTORY CULTURE CONSUMPTION
LA English
DT Article
DE luxury; Frasier; consumption; class identity; set design
AB Frasier was a widely successful American sitcom that centered around its luxurious main character Frasier Crane and his eccentric family. Much of the comedy focused on character quirks and family dynamics, but this article argues that the objects within the Crane world were just as essential and illuminating as the characters themselves. From the first episode the set was utilized as a physical embodiment of Frasier's identity and class, as well as the anxieties that ensued whenever his identity was threatened. Utilizing Grant McCracken's concept of the Diderot effect and Diderot unity it is possible to explore the sitcom in a manner that deftly highlights how easy and all-consuming it can be to build and protect one's identity through the meticulous consumption of specific possessions. In the end, we find that it is not only Frasier who falls victim to this connection between possessions and identity, but all of us. Much like the set is a reflection of who Frasier is, Frasier, the sitcom, becomes a reflection of the viewer and our culture at large.
C1 [Gibbons, Sarah] Copper Hewitt, Smithsonian Design Museum, New York, NY 10128 USA.
RP Gibbons, S (reprint author), Copper Hewitt, Smithsonian Design Museum, New York, NY 10128 USA.
EM sarah.reid086@gmail.com
NR 14
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2051-1817
EI 2051-1825
J9 LUX-HIST CULT CONSUM
JI Lux.-Hist. Cult. Consum.
PY 2016
VL 3
IS 1-2
BP 33
EP 46
DI 10.1080/20511817.2016.1232467
PG 14
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA EJ9UN
UT WOS:000393572700003
ER
PT S
AU Monsalve, C
Hazari, Z
McPadden, D
Sonnert, G
Sadler, PM
AF Monsalve, Camila
Hazari, Zahra
McPadden, Daryl
Sonnert, Gerhard
Sadler, Philip M.
BE Jones, DL
Ding, L
Traxler, A
TI Examining the Relationship between Career Outcome Expectations and
Physics Identity
SO 2016 PHYSICS EDUCATION RESEARCH CONFERENCE
SE Physics Education Research Conference
LA English
DT Proceedings Paper
CT Physics Education Research Conference (PERC)
CY JUL 20-21, 2016
CL Sacramento, CA
SP Amer Assoc Phys Teachers
ID MODEL; SCIENCE; CHOICE; WOMEN; EXPERIENCES; STUDENTS; GENDER
AB Previous studies about career outcome expectations, or what students hope to achieve in their careers, have revealed strong relationships between outcome expectations and STEM career choice. Drawing from a US national survey with responses from 15,847 students in mandatory College English courses (Outreach Programs and Science Career Intentions, NSF # 1161052), we examined the relationship between students outcome expectations and physics identity. It has previously been found that students with certain outcome expectations are more likely to develop a physics identity. Expanding beyond prior work, we focus on how outcome expectations are related to physics identity for students grouped by: (i) medical and engineering career aspirations, and (ii) female and male self-identification. The results provide a more nuanced understanding of the relationship between outcome expectations and physics identity for different students.
C1 [Monsalve, Camila; Hazari, Zahra; McPadden, Daryl] Florida Int Univ, Dept Phys, 11200 SW 8th St, Miami, FL 33199 USA.
[Hazari, Zahra] Florida Int Univ, Dept Teaching & Learning, 11200 SW 8th St, Miami, FL 33199 USA.
[Hazari, Zahra] Florida Int Univ, STEM Transformat Inst, 11200 SW 8th St, Miami, FL 33199 USA.
[Sonnert, Gerhard; Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA.
RP Monsalve, C (reprint author), Florida Int Univ, Dept Phys, 11200 SW 8th St, Miami, FL 33199 USA.
FU NSF [1161052]
FX This material is based upon work supported by NSF Grant No. 1161052. We
would like to thank the English professors and students who participated
as well as the OPSCI team.
NR 19
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC PHYSICS TEACHERS
PI COLLEGE PARK
PA ONE PHYSICS ELLIPSE, COLLEGE PARK, MD 20740-3845 USA
SN 2377-2379
BN 978-1-931024-30-3
J9 PHYS EDUC RES CONF
PY 2016
BP 228
EP 231
DI 10.1119/perc.2016.pr.052
PG 4
WC Education & Educational Research
SC Education & Educational Research
GA BG9CB
UT WOS:000393035800055
ER
PT J
AU Thurston, T
AF Thurston, Timothy
TI Rituals of Ethnicity: Thangmi Identities Between Nepal and India
SO ASIAN ETHNOLOGY
LA English
DT Book Review
C1 [Thurston, Timothy] Smithsonian Inst, Washington, DC 20560 USA.
RP Thurston, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU NANZAN UNIV, NANZAN INST RELIGION & CULTURE
PI NAGOYA
PA 18 YAMAZATO-CHO SHOWA-KU, NAGOYA, 466, JAPAN
SN 1882-6865
J9 ASIAN ETHNOL
JI Asian Ethnol.
PY 2016
VL 75
IS 2
BP 481
EP U402
PG 5
WC Folklore; Asian Studies
SC Arts & Humanities - Other Topics; Asian Studies
GA EJ3KD
UT WOS:000393110200014
ER
PT J
AU Carlson, SB
Blackman, MJ
Bishop, RL
AF Carlson, Shawn B.
Blackman, M. James
Bishop, Ronald L.
TI Texas Mission Ceramics: Origins of Manufacture and Distribution during
the Eighteenth Century
SO HISTORICAL ARCHAEOLOGY
LA English
DT Article
ID NEUTRON-ACTIVATION ANALYSIS; ARCHAEOLOGY
AB Nearly 800 ceramic sherds from 10 Spanish colonial sites in Texas were analyzed using instrumental neutron activation analysis (INAA) as a tool for understanding the local-resource production and distribution of Native American pottery, lead-glazed coarse earthenwares, and tin-glazed wares (majolica). The chemical characteristics of their pastes were compared to identify similarities that might indicate sources of manufacture. Data were also compared to other INAA studies. Combined with accounts of known supply stations and supply routes into Texas, the authors were able to identify three manufacturing locales for Native American pottery and five for lead-glazed wares. Evidence of a period of transition between Native American technologies and European technologies was also inferred.
C1 [Carlson, Shawn B.] Star Republ Museum, POB 317, Washington, TX 77880 USA.
[Blackman, M. James; Bishop, Ronald L.] Smithsonian Inst, Natl Museum Nat Hist, MRC112, Dept Anthropol, 10th & Constitut Ave NW, Washington, DC 20560 USA.
RP Carlson, SB (reprint author), Star Republ Museum, POB 317, Washington, TX 77880 USA.
NR 38
TC 0
Z9 0
U1 0
U2 0
PU SOC HISTORICAL ARCHAEOLOGY
PI ROCKVILLE
PA 9707 KEY WEST AVENUE, STE 100, ROCKVILLE, MD 20850 USA
SN 0440-9213
J9 HIST ARCHAEOL
JI Hist. Archaeol.
PY 2016
VL 50
IS 4
BP 65
EP 91
PG 27
WC Archaeology
SC Archaeology
GA EJ0MI
UT WOS:000392902800005
ER
PT J
AU Crampton, WGR
de Santana, CD
Waddell, JC
Lovejoy, NR
AF Crampton, William G. R.
de Santana, Carlos D.
Waddell, Joseph C.
Lovejoy, Nathan R.
TI A taxonomic revision of the Neotropical electric fish genus
Brachyhypopomus (Ostariophysi: Gymnotiformes: Hypopomidae), with
descriptions of 15 new species
SO NEOTROPICAL ICHTHYOLOGY
LA English
DT Article
DE Biogeography; Bluntnose knifefish; Electroreception; Identification key;
Rhamphichthyoidea
ID SOUTH-AMERICA GYMNOTIFORMES; FRESH-WATER FISHES; ORGAN DISCHARGE;
OCCIDENTALIS GYMNOTIFORMES; PINNICAUDATUS HYPOPOMIDAE; TUBEROUS
ELECTRORECEPTORS; ORDER GYMNOTIFORMES; FREQUENCY-RESPONSE;
SEXUAL-DIMORPHISM; PULSE DISCHARGE
AB The bluntnose knifefish genus Brachyhypopomus Mago-Leccia, 1994, is diagnosed from other Rhamphichthyoidea (Rhamphichthyidae + Hypopomidae) by the presence of a disk-like ossification in the anterior portion of the palatoquadrate, and by the following external characters: short snout, 18.7-32.6% of head length (vs. 33.3-68.6% in Hypopomus, Gymnorhamphichthys, Iracema, and Rhamphichthys), absence of a paired accessory electric organ in the mental or humeral region (vs. presence in Hypopygus and Steatogenys), presence of 3-4 pectoral proximal radials (vs. 5 in Akawaio), presence of the antorbital + infraorbital, and the preopercular cephalic lateral line canal bones (vs. absence in Racenisia). Brachyhypopomus cannot be diagnosed unambiguously from Microsternarchus or from Procerusternarchus on the basis of external characters alone. Brachyhypopomus comprises 28 species. Here we describe 15 new species, and provide redescriptions of all 13 previously described species, based on meristic, morphometric, and other morphological characters. We include notes on ecology and natural history for each species, and provide regional dichotomous keys and distribution maps, based on the examination of 12,279 specimens from 2,787 museum lots. A lectotype is designated for Brachyhypopomus pinnicaudatus (Hopkins, Comfort, Bastian & Bass, 1990). Brachyhypopomus species are abundant in shallow lentic and slow-flowing freshwater habitats from southern Costa Rica and northern Venezuela to Uruguay and northern Argentina. Species diversity is highest in Greater Amazonia, where 20 species occur: B. alberti, new species, B. arrayae, new species, and B. cunia, new species, in the upper rio Madeira drainage; B. batesi, new species, in the central Amazon and rio Negro; B. beebei, B. brevirostris, B. regani, new species, B. sullivani, new species, and B. walteri, widespread through the Amazon and Orinoco basins and the Guianas; B. belindae, new species, in the central Amazon basin; B. benjamini, new species, and B. verdii, new species, in the upper Amazon basin; B. bennetti, in the upper, central, and lower Amazon, lower Tocantins, and upper Madeira basins; B. bullocki in the Orinoco, Negro and Essequibo drainages; B. diazi in the Orinoco Llanos; B. flavipomus, new species, and B. hamiltoni, new species, in the central and upper Amazon basin; B. hendersoni, new species, in the central Amazon, lower Negro and Essequibo basins; B. pinnicaudatus in the central and lower Amazon, lower, upper Madeira, lower Tocantins and Mearim basins, and coastal French Guiana; and B. provenzanoi, new species, in the upper Orinoco and upper Negro basins. Five species are known from the Parana-Paraguay-Uruguay basin and adjacent southern Atlantic drainages: B. bombilla in the lower Parana, upper, central, and lower Paraguay, Uruguay and Patos-Mirim drainages; B. brevirostris in the upper Paraguay basin; B. draco in the lower Parana, lower Paraguay, Uruguay, Patos-Mirim, and Tramandai basins; B. gauderio in the lower Parana, upper, central, and lower Paraguay, Uruguay, Patos-Mirim and Tramandai basins; and B. walteri in the lower Parana and upper Paraguay basins. Two species occur in small Atlantic drainages of southern Brazil: B. janeiroensis in the Sao Joao, Paraiba and small intervening drainages; and B. jureiae in the Ribeira de Iguape and Una do Prelado. One species occurs in the middle and upper Sao Francisco basin: B. menezesi, new species. Three species occur in trans-Andean drainages: B. diazi in Caribbean drainages of northern Venezuela; B.
occidentalis in Atlantic and Pacific drainages of southern Costa Rica and Panama to Darien, and the Maracaibo, Magdalena, Sinu and Atrato drainages; and B. palenque, new species, in Pacific drainages of Ecuador.
C1 [Crampton, William G. R.; de Santana, Carlos D.; Waddell, Joseph C.] Univ Cent Florida, Dept Biol, POB 162368, Orlando, FL 32816 USA.
[de Santana, Carlos D.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, 10th & Constitut Ave NW, Washington, DC 20560 USA.
[Lovejoy, Nathan R.] Univ Toronto Scarborough, Dept Biol Sci, 1265 Mil Trail, Toronto, ON M1C 1A5, Canada.
RP Crampton, WGR (reprint author), Univ Cent Florida, Dept Biol, POB 162368, Orlando, FL 32816 USA.
EM crampton@ucf.edu; apteronotidae@ig.com.br; joecwaddell@knights.ucf.edu;
lovejoy@utsc.utoronto.ca
FU United States National Science Foundation [DEB-0215388, DEB-0614334,
DEB-1146374]; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico - Brazil [CNPq 38062/96-2, 381597/97-0]; Ministerio da
Ciencia, Tecnologia, Inovacoes e Comunicacoes - Brazil; Instituto de
Desenvolvimento Sustentavel Mamiraua - Brazil; Fisheries Society of the
British Isles; University of Oxford; University of Central Florida
(UCF); Crampton Lab (UCF); Canadian National Science and Engineering
Research Council (NSERC); NSF [DEB-0614334]
FX The following provided access to museum specimens and associated data:
Adriana Almiron (AI, MACN-ict); Barbara Brown, Scott Schaeffer (AMNH);
Kyle Luckenbill, John Lundberg, Mark Sabaj-Perez (ANSP); Jonathan
Armbruster, David Werneke (AUM); Oliver Crimmen, James Maclaine (BMNH);
David Catania, Mysi Hoang (CAS/SU); Mariana Arraya Borges, Mabel
Maldonado (CBF, UMSS); John Friel, Charles Dardia (CU); Mauro Triques
(DZUFMG); Susan Mochel, W. Leo Smith, Mark Westneat, Philip Willink
(FMNH); Javier Maldonado-Ocampo (CAC-CDMB/IAVHP/IMCN); Michael Retzer,
Chris Taylor, Rachel Vinsel (INHS); Carlos Araujo-Lima, Lana Brasil,
Efrem Ferreira, Lucia Rapp Py-Daniel, Jansen Zuanon (INPA); Sabrina
Owens, Andrew Bentley (KU); Rick Feeney (LACM); Francisco Provenzano,
Alberto Marcano (MBUCV-V); Donald Taphorn (MCNG); Carlos de Lucena,
Margarete Seixas de Lucena, Jose Pezzi da Silva, Roberto Reis (MCP);
Karsten Hartel, Andrew Williston (MCZ); Carlos Lasso (MHNLS); Romain
Causse, Philippe Keith, Beatrice Parisi, P. Pruvost (MNHN); Marcelo
Loureiro, Ana Silva (MNHN-Uruguay, ZVC-P); Marcelo Britto, Paulo Buckup
(MNRJ); Wolmar Wosiacki (MPEG); Ericka Correa Roldan, Hernan Ortega
(MUSM); Margaret Docker (MZF-Manitoba); Jose Figueiredo, Flavio Lima,
Osvaldo Oyakawa, Mario de Pinna (MZUSP); Gabriela Hogue (NCSM); Anja
Palandacic, Helmut Wellendorf (NMW); Erik Ahlander, Bodil Kajrup, Sven
Kullander, Anders Silfvergrip (NRM); Erika Carrera Garcia (QCAZ-I);
Martien van Oijen (RMNH); Mary Burridge, Erling Holm, Hernan
Lopez-Fernandez, Richard Winterbottom (ROM); Juan Bogota
(SINCHI-CIACOL); Eldredge Birmingham (STRI); Kevin Conway, Heather
Prestridge (TCWC); Dean Hendrickson, Jessica Rosales (TNHC); Larry Page,
Robert Robins (UF); Julia Giora, Luiz Malabarba (UFRGS); Ricardo
Campos-da-Paz (UFRJ); Luiz de Queiroz, Willian O'Hara, Adriana Ribeiro
(UFRO-I); William Fink, Douglas Nelson (UMMZ); Susan Jewett, Sandra
Raredon, Shirleen Smith, Erika Wilbur, Jeff Williams, Richard Vari
(USNM); Flora Fernandes, Lurdes Almeida-Toledo (Instituto de
Biociencias, Universidade de Sao Paulo); Isaac Isbrucker, Hielke
Praagman (ZMA); Fredy Nugra (ZOOA); Flavio Lima (ZUEC); Horst Wilkens
(ZMH). W. Crampton was funded by the United States National Science
Foundation (grants DEB-0215388, DEB-0614334, DEB-1146374, and
supplements), Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico - Brazil (grants CNPq 38062/96-2 & 381597/97-0), Ministerio
da Ciencia, Tecnologia, Inovacoes e Comunicacoes - Brazil, Instituto de
Desenvolvimento Sustentavel Mamiraua - Brazil, Fisheries Society of the
British Isles, The University of Oxford, and the University of Central
Florida (UCF). C. de Santana was funded by a post-doctoral fellowship at
the Crampton Lab (UCF). N. Lovejoy was funded by Canadian National
Science and Engineering Research Council (NSERC) Discovery grants and by
NSF grant DEB-0614334.; We are greatly indebted to the following for
providing assistance with field collections or for providing specimens:
Pedro Aguilera, James Albert, Jonas Alves Oliveira, Carlos Araujo-Lima,
Mariana Arraya, Jose Marcio Ayres, Maria Aldea Guevara, Joao Bastos,
Waldecy Bentes Monteiro, Eldredge Birmingham, Devin Bloom, Juan Bogota,
Kristen Brochu, Ricardo Campos-da-Paz, Angel Caputi, Adauto Cardoso,
Gilberto Castro, Wilmar Chaverra Salazar, Diego Cognato, Ericka Correa
Roldan, Ben Crampton, Danillo dos Santos, Flora Fernandes, Sat Gavassa,
Julia Giora, William Hamilton, Peter Henderson, Francesco Janzen,
Matthew Kolmann, Jeff Lambert, Kristy Lester, Flavio Lima, Hernan
Lopez-Fernandez, Nathan Lujan, Javier Maldonado-Ocampo, Jan Mol, Carmen
Montana, Cleusa Nagamachi, National Geographic Television, Ronald
Navarrette-Amaya, Fredy Nugra, Alex Orfinger, Hernan Ortega, Osvaldo
Oyakawa, Luiz Queiroz, Jonathan Ready, Roberto Reis, Mathilde
Richer-de-Forges, Alejo Rodriguez-Cattaneo, Mark Sabaj-Perez, Ana Silva,
Charles Smyth, John Stark, Phillip Stoddard, Lorgio Verdi, Kenneth Wang
Tong You, Stuart Willis. Richard Crampton translated taxonomic papers
from German. Adrian Urquiola built the GIS system for the maps. For
fruitful discussions we thank James Albert, Gloria Arratia, Angel
Caputi, Hernan Fernandez-Lopez, Julia Giora, Carl Hopkins, Flavio Lima,
Javier Maldonado-Ocampo, Cleusa Nagamachi, Roberto Reis, Phillip
Stoddard, John Sullivan, Mauro Triques, Richard Vari, and Harold Zakon.
NR 208
TC 0
Z9 0
U1 2
U2 2
PU SOC BRASILEIRA ICTIOLOGIA
PI SAO PAULO
PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO
PAULO, SP 05508-900, BRAZIL
SN 1679-6225
J9 NEOTROP ICHTHYOL
JI Neotrop. Ichthyol.
PY 2016
VL 14
IS 4
AR e150146
DI 10.1590/1982-0224-20150146
PG 152
WC Zoology
SC Zoology
GA EJ2RN
UT WOS:000393058600003
ER
PT J
AU Doring, B
Mecke, S
Mader, F
Kaiser, H
AF Doering, Britta
Mecke, Sven
Mader, Felix
Kaiser, Hinrich
TI A proposed optimal incision method to obtain gut contents from preserved
anurans
SO AMPHIBIA-REPTILIA
LA English
DT Article
DE anatomy; Anura; food spectrum analysis; gut content analysis; incision;
invasive method
ID AMPHIBIA ANURA; DIET; BRAZIL
AB Information on the diet of anuran species based on gut content analyses have been published by numerous researchers, yet the details of the incision method used to open the abdominal cavity of preserved specimens in preparation for such examinations are rarely explained in the presented methods. Our objective is to formally propose an optimal incision into the pleuroperitoneal cavity of liquid-preserved anuran specimens to gain access to and permit easy removal of parts of the digestive tract in preparation for food spectrum analyses. In our experience, this U-shaped cut is easy to perform and teach. It also provides better access to the pleuroperitoneal cavity than a small ventrolateral incision and is less destructive than the classic textbook medial "double T-incision" routinely listed in dissection protocols.
C1 [Doering, Britta; Mecke, Sven] Philipps Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat & Zool Collect Marbur, Karl von Frisch Str 8, D-35032 Marburg, Germany.
[Mader, Felix] Janusstr 5, D-93051 Regensburg, Germany.
[Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA.
[Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP Mecke, S (reprint author), Philipps Univ Marburg, Fac Biol, Dept Anim Evolut & Systemat & Zool Collect Marbur, Karl von Frisch Str 8, D-35032 Marburg, Germany.
EM meckes@staff.uni-marburg.de
NR 23
TC 0
Z9 0
U1 0
U2 0
PU BRILL ACADEMIC PUBLISHERS
PI LEIDEN
PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS
SN 0173-5373
EI 1568-5381
J9 AMPHIBIA-REPTILIA
JI Amphib. Reptil.
PY 2016
VL 37
IS 4
BP 437
EP 440
DI 10.1163/15685381-00003061
PG 4
WC Zoology
SC Zoology
GA EI8GO
UT WOS:000392744300010
ER
PT J
AU O'Shea, M
Kaiser, H
AF O'Shea, Mark
Kaiser, Hinrich
TI The first female specimen of the poorly known Arfak Stouttailed Snake,
Calamophis sharonbrooksae Murphy, 2012 (Serpentes: Colubroidea:
Homalopsidae), from the Vogelkop Peninsula of Indonesian West New
Guinea, with comments on the taxonomic history of primitive homalopsids
SO AMPHIBIAN & REPTILE CONSERVATION
LA English
DT Article
DE Homalopsidae; Calamophis sharonbrooksae; Brachyorrhos; West Papua
Province; Vogelkop Peninsula
ID TIMOR-LESTE; TAILED SNAKES; SQUAMATA; HERPETOFAUNA; GENUS; PHYLOGENY;
MEYER; KEY
AB The recent resurrection of Calamophis Meyer, 1874, type species C. jobiensis, from the synonymy of Brachyorrhos Kuhl in Schlegel, 1826, and the description of three new species of Calamophis, have changed concepts of homalopsid diversity in the Vogelkop Peninsula of West New Guinea. Both Brachyorrhos and Calamophis are now accepted to comprise four species each and are considered representatives of a unique fangless, nonvenomous, terrestrial to semi-fossorial, homalopsid lineage. With the original and only specimen of C. jobiensis lost, the genus Calamophis is now characterized by only six specimens (4 male male, 2 female female), comprising holotypes and paratypes of the remaining three species; in each case the species is defined only by specimens of a single sex. We here present the description of the first female specimen of C. sharonbrooksae, the largest specimen of the genus discovered so far, which exhibits a slightly longer body (96% of SVL vs. 91%) and a higher ventral scale count (158 vs. 149 or 150) than the two males, combined with a significantly shorter tail (4.4% of total length vs. 8.6%) and a lower subcaudal scale count (12 pairs vs. 17 or 19 pairs). This is the first time both sexes of a Calamophis species have been available for comparison. The specimen is also the first mainland Papuan Calamophis documented outside the administrative boundaries of the Manokwari Residency, suggesting a wider distribution for the genus than previously thought.
C1 [O'Shea, Mark] Wolverhampton Univ, Fac Sci & Engn, Wulfruna St, Wolverhampton WV1 1LY, W Midlands, England.
[O'Shea, Mark] West Midland Safari Pk, Bewdley DY12 1LF, Worcs, England.
[Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA.
[Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP O'Shea, M (reprint author), Wolverhampton Univ, Fac Sci & Engn, Wulfruna St, Wolverhampton WV1 1LY, W Midlands, England.; O'Shea, M (reprint author), West Midland Safari Pk, Bewdley DY12 1LF, Worcs, England.
EM oshea@markoshea.info; hinrich.kaiser@vvc.edu
NR 49
TC 0
Z9 0
U1 0
U2 0
PU AMPHIBIAN & REPTILE CONSERVATION
PI MODESTO
PA 2525 IOWA AVE, MODESTO, CA 95358-9467 USA
SN 1083-446X
J9 AMPHIB REPTILE CONSE
JI Amphib. Reptile Conserv.
PY 2016
VL 10
IS 2
BP 1
EP 10
AR e122
PG 10
WC Zoology
SC Zoology
GA EI8GD
UT WOS:000392743100001
ER
PT S
AU Jian, LK
Moya, PS
Vinas, AF
Stevens, M
AF Jian, L. K.
Moya, P. S.
Vinas, A. F.
Stevens, M.
BE Wang, L
Bruno, R
Mobius, E
Vourlidas, A
Zank, G
TI Electromagnetic Cyclotron Waves in the Solar Wind: Wind Observation and
Wave Dispersion Analysis
SO PROCEEDINGS OF THE FOURTEENTH INTERNATIONAL SOLAR WIND CONFERENCE (SOLAR
WIND 14)
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 14th International Solar Wind Conference (Solar Wind)
CY JUN 22-26, 2015
CL Peking Univ, Sch Earth & Space Sci, Weihai, PEOPLES R CHINA
SP Shandong Univ, Inst Space Sci, Natl Nat Sci Fdn China, Chinese Acad Sci, Natl Space Sci Ctr, Beihang Univ
HO Peking Univ, Sch Earth & Space Sci
ID KINETIC SCALES; PROTON SCALES; 1 AU; FLUCTUATIONS; TURBULENCE; STEREO
AB Wind observed long-lasting electromagnetic cyclotron waves near the proton cyclotron frequency on 11 March 2005, in the descending part of a fast wind stream. Bi-Maxwellian velocity distributions are fitted for core protons, beam protons, and alpha-particles. Using the fitted plasma parameters we conduct kinetic linear dispersion analysis and find ion cyclotron and/or firehose instabilities grow in six of 10 wave intervals. After Doppler shift, some of the waves have frequency and polarization consistent with observation, thus may be correspondence to the cyclotron waves observed.
C1 [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jian, L. K.; Moya, P. S.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Moya, P. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Moya, P. S.] Univ Chile, Dept Fis, Santiago, Chile.
[Stevens, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM lan.jian@nasa.gov
RI Moya, Pablo/C-3163-2011
OI Moya, Pablo/0000-0002-9161-0888
FU NASA [NNX13AI65G, NNX15AB75G]
FX The work is supported by NASA under Awards NNX13AI65G and NNX15AB75G. We
thank the Wind mission team for making the data publically available.
NR 18
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U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-1367-2
J9 AIP CONF PROC
PY 2016
VL 1720
AR 040007
DI 10.1063/1.4943818
PG 4
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA BG8RW
UT WOS:000392692000018
ER
PT S
AU Slavin, JD
AF Slavin, Jonathan D.
BE Wang, L
Bruno, R
Mobius, E
Vourlidas, A
Zank, G
TI The Outer Boundary Conditions of the Heliosphere: Observations and
Models of the Local Interstellar Cloud
SO PROCEEDINGS OF THE FOURTEENTH INTERNATIONAL SOLAR WIND CONFERENCE (SOLAR
WIND 14)
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 14th International Solar Wind Conference (Solar Wind)
CY JUN 22-26, 2015
CL Peking Univ, Sch Earth & Space Sci, Weihai, PEOPLES R CHINA
SP Shandong Univ, Inst Space Sci, Natl Nat Sci Fdn China, Chinese Acad Sci, Natl Space Sci Ctr, Beihang Univ
HO Peking Univ, Sch Earth & Space Sci
ID NEUTRAL HELIUM; IBEX; PARAMETERS; FLOW; TEMPERATURES; IONIZATION;
MORPHOLOGY; DENSITIES; BUBBLE; GHRS
AB The outer boundary conditions of the heliosphere are set by the circumheliospheric interstellar medium, which is part of the Local Interstellar Cloud (LIC). In particular the ram pressure, ionization and magnetic field strength are important for determining the size and shape of the heliosphere. The in situ as well as line of sight data indicate that the LIC is a warm, partially ionized cloud. We discuss the observational evidence on the nature of the LIC and theoretical models that explain its temperature and ionization.
C1 [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 83, Cambridge, MA 02138 USA.
EM jslavin@cfa.harvard.edu
OI Slavin, Jonathan/0000-0002-7597-6935
FU Space Telescope Science Institute [GO-12981.01-A]; NASA Astrophysics
Theory Grant [NNX15AI60G]
FX The author wishes to acknowledge his collaborators for valuable
discussions, in particular. Priscilla C. Frisch, with whom much of the
work on the ionization of the LIC was carried out; Nicolas Lehner, PI on
the HST GO program to observe Sirius B; and Cecile Gry who fit the
Sirius data to determine the absorption line parameters and also created
the figure of the absorption line data and fit presented here. This work
was supported by grant No. GO-12981.01-A from the Space Telescope
Science Institute and NASA Astrophysics Theory Grant NNX15AI60G. The
author thanks the conference organizers for the invitation to give this
talk.
NR 23
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U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-1367-2
J9 AIP CONF PROC
PY 2016
VL 1720
AR 080003
DI 10.1063/1.4943852
PG 6
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA BG8RW
UT WOS:000392692000051
ER
PT J
AU Blersch, DM
Kangas, PC
Adey, WH
AF Blersch, D. M.
Kangas, P. C.
Adey, W. H.
TI FRESHWATER MARSH COMMUNITY STRUCTURE IN A FLORIDA EVERGLADES MESOCOSM
SO Transactions of the ASABE
LA English
DT Article
DE Cladium; Competition; Everglades; Freshwater marsh; Mesocosm; Nutrients;
Typha
ID CLADIUM-JAMAICENSE CRANTZ; TYPHA-DOMINGENSIS PERS; PHOSPHORUS
ENRICHMENT; ABOVEGROUND BIOMASS; DECOMPOSITION; VEGETATION; NUTRIENTS;
RESTORATION; ECOSYSTEMS; PERIPHYTON
AB Considerable research activity has been undertaken to characterize the effects of nutrient cycle changes on the distribution of plant communities in the Florida Everglades. Studies of constructed Everglades ecosystems at the mesocosm scale offer avenues for researching the complexities of these interactions. The objectives of this study were to describe the vegetation that developed in the Florida Everglades mesocosm in Washington, D.C., a greenhouse-sized constructed Everglades ecosystem in operation from 1987 to 2001. Literature on actual Everglades vegetation was used to make comparisons with the vegetation in the mesocosm. The entire standing herbaceous biomass was harvested from the mesocosm's cattail and sawgrass communities, and samples of belowground biomass were taken from various points throughout. Dry weights of the samples revealed the highest overall aboveground biomass (2223 g m(-2)) in the mixed cattail/sawgrass community of the emergent marsh/herbaceous hummock section, and the lowest (1302 g m(-2)) in the grass prairie. The highest belowground biomass (4058 g m(-2)) was also found in the marsh/hummock, and the lowest (64 g m(-2)) was found in the marsh/pond. These biomass values fall within the ranges found in the literature on productivity of cattail and sawgrass communities. The distribution of the plant species fluctuated between the community sections, with species richness highest in the grass prairie and lowest in the marsh/pond. The fluctuations of plant assemblages between the community sections give evidence that the sections may represent the transition zone between tree islands and sawgrass marsh communities found in the wild. Soil and leaf nutrient contents were within expected ranges of their natural analogs, although no significant differences were seen between the cattail and sawgrass populations. Artifacts of the mesocosm were strongly evident, such as edge effects in community density, yet the ecological structure of the mesocosm was strikingly close to that found in the wild Everglades. Overall, the experience with the management, harvest, and study of the Florida Everglades mesocosm demonstrates the value of large-scale mesocosm studies for representation of ecological structures and functions.
C1 [Blersch, D. M.] Auburn Univ, Dept Biosyst Engn, Auburn, AL 36849 USA.
[Kangas, P. C.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA.
[Adey, W. H.] Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA.
RP Blersch, DM (reprint author), Auburn Univ, 203 Tom Corley Bldg, Auburn, AL 36849 USA.
EM dmb0040@auburn.edu
NR 52
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Z9 1
U1 0
U2 0
PU AMER SOC AGRICULTURAL & BIOLOGICAL ENGINEERS
PI ST JOSEPH
PA 2950 NILES RD, ST JOSEPH, MI 49085-9659 USA
SN 2151-0032
EI 2151-0040
J9 T ASABE
JI Trans. ASABE
PY 2016
VL 59
IS 5
BP 1305
EP 1312
DI 10.13031/trans.59.11599
PG 8
WC Agricultural Engineering
SC Agriculture
GA EJ0VP
UT WOS:000392929300028
ER
PT S
AU Cotroneo, V
Allured, R
Reid, PB
Deroo, CT
Schwartz, DA
Marquez, V
Vikhlinin, AA
Civitani, M
Salmaso, B
Pareschi, G
AF Cotroneo, Vincenzo
Allured, Ryan
Reid, Paul B.
DeRoo, Casey T.
Schwartz, Daniel A.
Marquez, Vanessa
Vikhlinin, Alexey A.
Civitani, Marta
Salmaso, Bianca
Pareschi, Giovanni
BE ODell, SL
Khounsary, AM
TI Thermal Forming of Substrates for the X-Ray Surveyor Telescope
SO ADAPTIVE X-RAY OPTICS IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Adaptive X-Ray Optics IV as part of the SPIE Optics +
Photonics International Symposium on Optical Engineering + Applications
CY AUG 28-29, 2016
CL San Diego, CA
SP SPIE Opt + Photon
DE X-ray grazing incidence telescopes; Wolter mirrors; glass slumping;
thermal forming
AB In this paper we review the progress and current status of thermal forming activities at SAO, highlighting the most relevant technical problems and the way to solve them. These activities are devoted to the realization of mirror substrates for the X-ray surveyor mission concept, an observatory with Chandra-like angular resolution and 30 times more effective area or larger. The technology under development at SAO is based on the deposition of piezoelectric material on the back of the substrates. About 8000 mirror segments, with initial quality of 10 arcseconds or better are required for the telescope.
C1 [Cotroneo, Vincenzo; Allured, Ryan; Reid, Paul B.; DeRoo, Casey T.; Schwartz, Daniel A.; Marquez, Vanessa; Vikhlinin, Alexey A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Civitani, Marta; Salmaso, Bianca; Pareschi, Giovanni] Osserv Astron Brera, Via Bianchi 46, Merate, LC, Italy.
RP Cotroneo, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM vcotroneo@cfa.harvard.edu
FU NASA [NNX13AD46G, NNX15AC44G]; National Science Foundation [1541959]
FX This work was supported by NASA Contracts NNX13AD46G and NNX15AC44G, and
also by internal Smithsonian funding. It was performed in part at the
Center for Nanoscale Systems (CNS), a member of the National
Nanotechnology Coordinated Infrastructure Network (NNCI), which is
supported by the National Science Foundation under NSF award no.
1541959. CNS is part of Harvard University.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0321-9; 978-1-5106-0322-6
J9 PROC SPIE
PY 2016
VL 9965
AR UNSP 99650C
DI 10.1117/12.2239223
PG 6
WC Optics; Physics, Applied
SC Optics; Physics
GA BG8GQ
UT WOS:000392269700009
ER
PT S
AU O'Dell, SL
Allured, R
Ames, AO
Biskach, MP
Broadway, DM
Bruni, RJ
Burrows, DN
Cao, J
Chalifoux, BD
Chan, KW
Chung, YW
Cotroneo, V
Elsner, RF
Gaskin, JA
Gubarev, MV
Heilmann, RK
Hertz, E
Jackson, TN
Kilaru, K
Kolodziejczak, JJ
McClelland, RS
Ramsey, BD
Reid, PB
Riveros, RE
Roche, JM
Romaine, SE
Saha, TT
Schattenburg, ML
Schwartz, DA
Schwartz, ED
Solly, PM
Trolier-McKinstry, SE
Ulmer, MP
Vikhlinin, A
Wallace, ML
Wang, XL
Windt, DL
Yao, YW
Ye, S
Zhang, WW
Zuo, H
AF O'Dell, Stephen L.
Allured, Ryan
Ames, Andrew O.
Biskach, Michael P.
Broadway, David M.
Bruni, Ricardo J.
Burrows, David N.
Cao, Jian
Chalifoux, Brandon D.
Chan, Kai-Wing
Chung, Yip-Wah
Cotroneo, Vincenzo
Elsner, Ronald F.
Gaskin, Jessica A.
Gubarev, Mikhail V.
Heilmann, Ralf K.
Hertz, Edward
Jackson, Thomas N.
Kilaru, Kiranmayee
Kolodziejczak, Jeffery J.
McClelland, Ryan S.
Ramsey, Brian D.
Reid, Paul B.
Riveros, Raul E.
Roche, Jacqueline M.
Romaine, Suzanne E.
Saha, Timo T.
Schattenburg, Mark L.
Schwartz, Daniel A.
Schwartz, Eric D.
Solly, Peter M.
Trolier-McKinstry, Susan E.
Ulmer, Melville P.
Vikhlinin, Alexey
Wallace, Margeaux L.
Wang, Xiaoli
Windt, David L.
Yao, Youwei
Ye, Shi
Zhang, William W.
Zuo, Heng
BE ODell, SL
Khounsary, AM
TI Toward large-area sub-arcsecond x-ray telescopes II
SO ADAPTIVE X-RAY OPTICS IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Adaptive X-Ray Optics IV as part of the SPIE Optics +
Photonics International Symposium on Optical Engineering + Applications
CY AUG 28-29, 2016
CL San Diego, CA
SP SPIE Opt + Photon
DE X-ray telescopes; x-ray optics; slumped-glass mirrors; silicon mirrors;
differential deposition; coating stress; ion implantation; active
optics; electro-active devices; magneto-active devices
ID MIRRORS; DEPOSITION
AB In order to advance significantly scientific objectives, future x-ray astronomy missions will likely call for x-ray telescopes with large aperture areas (approximate to 3 m(2)) and fine angular resolution (approximate to 1 ''). Achieving such performance is programmatically and technologically challenging due to the mass and envelope constraints of space-borne telescopes and to the need for densely nested grazing-incidence optics. Such an x-ray telescope will require precision fabrication, alignment, mounting, and assembly of large areas (approximate to 600 m(2)) of lightweight (approximate to 2 kg/m(2) areal density) high-quality mirrors, at an acceptable cost (approximate to 1 M$/m(2) of mirror surface area). This paper reviews relevant programmatic and technological issues, as well as possible approaches for addressing these issues-including direct fabrication of monocrystalline silicon mirrors, active (in-space adjustable) figure correction of replicated mirrors, static post-fabrication correction using ion implantation, differential erosion or deposition, and coating-stress manipulation of thin substrates.
C1 [O'Dell, Stephen L.; Broadway, David M.; Elsner, Ronald F.; Gaskin, Jessica A.; Gubarev, Mikhail V.; Kolodziejczak, Jeffery J.; Ramsey, Brian D.; Roche, Jacqueline M.] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Allured, Ryan; Ames, Andrew O.; Bruni, Ricardo J.; Cotroneo, Vincenzo; Hertz, Edward; Reid, Paul B.; Romaine, Suzanne E.; Schwartz, Daniel A.; Schwartz, Eric D.; Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Biskach, Michael P.; McClelland, Ryan S.; Solly, Peter M.] Stinger Ghaffarian Technol Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burrows, David N.; Jackson, Thomas N.; Trolier-McKinstry, Susan E.; Wallace, Margeaux L.] Penn State Univ, University Pk, PA 16802 USA.
[Cao, Jian; Chung, Yip-Wah; Ulmer, Melville P.; Wang, Xiaoli; Yao, Youwei; Ye, Shi] Northwestern Univ, Evanston, IL 60208 USA.
[Chalifoux, Brandon D.; Heilmann, Ralf K.; Schattenburg, Mark L.; Yao, Youwei; Zuo, Heng] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Chan, Kai-Wing; Riveros, Raul E.] Univ Maryland Baltimore Co, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kilaru, Kiranmayee] Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Saha, Timo T.; Zhang, William W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Windt, David L.] Reflect Xray Opt LLC, New York, NY 10027 USA.
RP O'Dell, SL (reprint author), NASA MSFC ZP 12, 320 Sparkman Dr NW, Huntsville, AL 35805 USA.
EM stephen.l.odell@nasa.gov
NR 67
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U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0321-9; 978-1-5106-0322-6
J9 PROC SPIE
PY 2016
VL 9965
AR UNSP 996507
DI 10.1117/12.2238247
PG 17
WC Optics; Physics, Applied
SC Optics; Physics
GA BG8GQ
UT WOS:000392269700005
ER
PT J
AU Londt, JGH
Dikow, T
AF Londt, Jason G. H.
Dikow, Torsten
TI A review of the genus Trichoura Londt, 1994 with the description of a
new species from the Northern Cape Province of South Africa and a key to
world Willistonininae (Diptera, Asilidae)
SO AFRICAN INVERTEBRATES
LA English
DT Article
DE Assassin flies; robber flies; Afrotropical; Nearctic; new tribe; new
species
ID BRACHYCERA ASILOIDEA; STENOPOGONINAE; GENERA
AB The South African assassin-fly genus Trichoura Londt, 1994 is reviewed. A new species, Trichoura pardeos sp. n., is described from the arid Karoo in north-western South Africa. A new key to all seven recognized species is provided and the distribution and phenology are discussed. The world fauna of Willistonininae is reviewed, a new taxon Sisyrnodytini tribe n. (type genus Sisyrnodytes Loew, 1856) is established for Ablautus Loew, 1866, Acnephalomyia Londt, 2010, Ammodaimon Londt, 1985, Astiptomyia Londt, 2010, Sisyrnodytes, and Sporadothrix Hermann, 1908 and photographs for all Willistonininae genera are provided.
C1 [Londt, Jason G. H.] KwaZulu Natal Museum, P Bag 9070, ZA-3200 Pietermaritzburg, South Africa.
[Londt, Jason G. H.] Univ KwaZulu Natal, Sch Biol & Conservat Sci, Pietermaritzburg, South Africa.
[Dikow, Torsten] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Dikow, T (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM dikowt@si.edu
OI Dikow, Torsten/0000-0003-4816-2909
FU University of KwaZulu-Natal; National Research Foundation (NRF) of South
Africa
FX The senior author wishes to thank the University of KwaZulu-Natal and
the National Research Foundation (NRF) of South Africa for allocating
funding in support of his research. The KwaZulu-Natal Museum provided
various services while his wife, Ann, continued to provide assistance
and support. The junior author acknowledges field work support by the
Global Genome Initiative (GGI) at the Smithsonian Institution to visit
the Nama and Klein Karoo in December 2015. The team at the De Zeekoe
Guest Farm and in particular Dolf Grobler and J.D. Glinister are thanked
for allowing collecting and accompanying the junior author in the field.
Karie Darrow and Meg Gisonda are thanked for assistance in photographing
specimens. Rodrigo Vieira and Aubrey Scarbrough are thanked for comments
that improved the manuscript during peer review. The assistance of the
conservation authorities issuing collecting permits in the Northern Cape
and Western Cape Provinces is appreciated.
NR 13
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U1 0
U2 0
PU COUNCIL NATAL MUSEUM
PI PIETERMARITZBURG
PA PRIVATE BAG 9070, PIETERMARITZBURG, KWAZULU-NATAL 00000, SOUTH AFRICA
SN 1681-5556
EI 2305-2562
J9 AFR INVERTEBR
JI Afr. Invertebr.
PY 2016
VL 57
IS 2
SI SI
BP 119
EP 135
DI 10.3897/AfrInvertebr.57.10772
PG 17
WC Entomology; Paleontology; Zoology
SC Entomology; Paleontology; Zoology
GA EI7GZ
UT WOS:000392667100005
ER
PT S
AU Ben-Ami, S
Epps, H
Evans, I
Mueller, M
Podgorski, W
Szentgyorgyi, A
AF Ben-Ami, Sagi
Epps, Harland
Evans, Ian
Mueller, Mark
Podgorski, William
Szentgyorgyi, Andrew
BE Evans, CJ
Simard, L
Takami, H
TI The optical design of the G-CLEF Spectrograph: the first light
instrument for the GMT
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE GMT; ELT; Echelle; Spectrographs; PRV; Exoplanets
AB The GMT-Consortium Large Earth Finder (G-CLEF), the first major light instrument for the GMT, is a fiber-fed, high-resolution echelle spectrograph. In the following paper, we present the optical design of G-CLEF. We emphasize the unique solutions derived for the spectrograph fiber-feed: the Mangin mirror that corrects the cylindrical field curvature, the implementation of VPH grisms as cross dispersers, and our novel solution for a multi-colored exposure meter. We describe the spectrograph blue and red cameras comprised of 7 and 8 elements respectively, with one aspheric surface in each camera, and present the expected echellogram imaged on the instrument focal planes. Finally, we present ghost analysis and mitigation strategy that takes into account both single reflection and double reflection back scattering from various elements in the optical train.
C1 [Ben-Ami, Sagi; Evans, Ian; Mueller, Mark; Podgorski, William; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
[Epps, Harland] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP Ben-Ami, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
NR 12
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 9908A0
DI 10.1117/12.2232854
PG 16
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100278
ER
PT S
AU Crepp, JR
Crass, J
King, D
Bechter, A
Bechter, E
Ketterer, R
Reynold, R
Hinz, P
Kopon, D
Cavalieri, D
Fantano, L
Koca, C
Onuma, E
Stapelfeldt, K
Thomes, J
Wall, S
Macenka, S
McGuire, J
Komiski, R
Zugby, L
Eisner, J
Gaudi, BS
Hearty, F
Kratter, K
Kuchner, M
Micela, G
Nelson, M
Pagano, I
Quirrenbach, A
Schwab, C
Skrutskie, M
Sozzetti, A
Woodward, CE
Zhao, B
AF Crepp, Justin R.
Crass, Jonathan
King, David
Bechter, Andrew
Bechter, Eric
Ketterer, Ryan
Reynold, Robert
Hinz, Philip
Kopon, Derek
Cavalieri, David
Fantano, Louis
Koca, Corina
Onuma, Eleanya
Stapelfeldt, Karl
Thomes, Joseph
Wall, Sheila
Macenka, Steven
McGuire, James
Komiski, Ronald
Zugby, Leonard
Eisner, Joshua
Gaudi, B. Scott
Hearty, Fred
Kratter, Kaitlin
Kuchner, Marc
Micela, Giusi
Nelson, Matthew
Pagano, Isabella
Quirrenbach, Andreas
Schwab, Christian
Skrutskie, Michael
Sozzetti, Alessandro
Woodward, Charles E.
Zhao, Bo
BE Evans, CJ
Simard, L
Takami, H
TI iLocater: A Diffraction-limited Doppler Spectrometer for the Large
Binocular Telescope
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE spectroscopy; exoplanets; radial velocity; optical fibers; adaptive
optics
AB We are developing a stable and precise spectrograph for the Large Binocular Telescope (LBT) named "iLocater." The instrument comprises three principal components: a cross-dispersed echelle spectrograph that operates in the YJ-bands (0.97-1.30 mu m), a fiber-injection acquisition camera system, and a wavelength calibration unit. iLocater will deliver high spectral resolution (R similar to 150,000-240,000) measurements that permit novel studies of stellar and substellar objects in the solar neighborhood including extrasolar planets. Unlike previous planet-finding instruments, which are seeing-limited, iLocater operates at the diffraction limit and uses single mode fibers to eliminate the effects of modal noise entirely. By receiving starlight from two 8.4m diameter telescopes that each use "extreme" adaptive optics (AO), iLocater shows promise to overcome the limitations that prevent existing instruments from generating sub-meter-per-second radial velocity (RV) precision. Although optimized for the characterization of low-mass planets using the Doppler technique, iLocater will also advance areas of research that involve crowded fields, line-blanketing, and weak absorption lines.
C1 [Crepp, Justin R.; Crass, Jonathan; Bechter, Andrew; Bechter, Eric; Ketterer, Ryan; Cavalieri, David] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA.
[King, David] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England.
[Reynold, Robert] Large Binocular Telescope Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Hinz, Philip; Eisner, Joshua; Kratter, Kaitlin] Univ Arizona, Steward Observ, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Kopon, Derek] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fantano, Louis; Koca, Corina; Onuma, Eleanya; Stapelfeldt, Karl; Thomes, Joseph; Wall, Sheila; Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stapelfeldt, Karl; Macenka, Steven; McGuire, James; Komiski, Ronald; Zugby, Leonard] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gaudi, B. Scott] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Hearty, Fred] Penn State Univ, Davey Lab 405, University Pk, PA 16802 USA.
[Micela, Giusi] Osservatrio Astron Paleuno GS Vaiana, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Nelson, Matthew] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Pagano, Isabella] Osserv Astrofis Catania, INAF, Via S Sofia78, I-95123 Catania, Italy.
[Quirrenbach, Andreas] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Schwab, Christian] Macquarie Univ, Sydney, NSW 2109, Australia.
[Schwab, Christian] Australian Astron Observ, Sydney, NSW, Australia.
[Sozzetti, Alessandro] Osserv Astron Torino, INAF, Via Osservat 20, I-10025 Pino Torinese, Italy.
[Woodward, Charles E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St,SE, Minneapolis, MN 55455 USA.
[Zhao, Bo] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
RP Crepp, JR (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 990819
DI 10.1117/12.2233135
PG 13
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100032
ER
PT S
AU Crouzet, N
Mekarnia, D
Guillot, T
Abe, L
Agabi, A
Rivet, JP
Goncalves, I
Schmider, FX
Daban, JB
Fantei-Caujolle, Y
Gouvret, C
Bayliss, DDR
Zhou, G
Aristidi, E
Fruth, T
Erikson, A
Rauer, H
Szulagyi, J
Bondoux, E
Challita, Z
Pouzenc, C
Fressin, F
Valbousquet, F
Barbieri, M
Blazit, A
Bonhomme, S
Bouchy, F
Gerakis, J
Bouchez, G
AF Crouzet, N.
Mekarnia, D.
Guillot, T.
Abe, L.
Agabi, A.
Rivet, J. -P.
Goncalves, I.
Schmider, F. -X.
Daban, J. -B.
Fantei-Caujolle, Y.
Gouvret, C.
Bayliss, D. D. R.
Zhou, G.
Aristidi, E.
Fruth, T.
Erikson, A.
Rauer, H.
Szulagyi, J.
Bondoux, E.
Challita, Z.
Pouzenc, C.
Fressin, F.
Valbousquet, F.
Barbieri, M.
Blazit, A.
Bonhomme, S.
Bouchy, F.
Gerakis, J.
Bouchez, G.
BE Evans, CJ
Simard, L
Takami, H
TI Six winters of photometry from Dome C, Antarctica: challenges,
improvements, and results from the ASTEP experiment
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Photometry; Exoplanets; Dome C; Antarctica
ID SEARCH; TELESCOPE; CONCORDIA; LAYER
AB ASTEP (Antarctica Search for Transiting ExoPlanets) is a pilot project that aims at searching and characterizing transiting exoplanets from Dome C in Antarctica and to qualify this site for photometry in the visible. Two instruments were installed at Dome C and ran for six winters in total. The analysis of the collected data is nearly complete. We present the operation of the instruments, and the technical challenges, limitations, and possible solutions in light of the data quality. The instruments performed continuous observations during the winters. Human interventions are required mainly for regular inspection and ice dust removal. A defrosting system is efficient at preventing and removing ice on the mirrors. The PSF FWHM is 4.5 arcsec on average which is 2.5 times larger than the specification, and is highly variable; the causes are the poor ground-level seeing, the turbulent plumes generated by the heating system, and to a lower extent the imperfect optical alignment and focusing, and some astigmatism. We propose solutions for each of these aspects that would largely increase the PSF stability. The astrometric and guiding precisions are satisfactory and would deserve only minor improvements. Major issues are encountered with the camera shutter which did not close properly after two winters; we minimized this issue by heating the shutter and by developing specific image calibration algorithms. Finally, we summarize the site testing and science results obtained with ASTEP. Overall, the ASTEP experiment will serve as a basis to design and operate future optical and near-infrared telescopes in Antarctica.
C1 [Crouzet, N.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Mekarnia, D.; Guillot, T.; Abe, L.; Agabi, A.; Rivet, J. -P.; Goncalves, I.; Schmider, F. -X.; Daban, J. -B.; Fantei-Caujolle, Y.; Gouvret, C.; Aristidi, E.; Bondoux, E.; Blazit, A.; Bonhomme, S.; Gerakis, J.] Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Bayliss, D. D. R.] Observ Univ Geneve, 51 Chemin Maillettes, CH-1290 Sauverny, Switzerland.
[Zhou, G.; Fressin, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fruth, T.; Erikson, A.; Rauer, H.] Deutsch Zentrum Luftund Raumfahrt, Inst Planetenforsch, Rutherfordstr 2, D-12489 Berlin, Germany.
[Fruth, T.] German Aerosp Ctr, Germany Space Operat Ctr, Munchener Str 20, D-82234 Wessling, Germany.
[Rauer, H.] Tech Univ Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany.
[Szulagyi, J.] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Challita, Z.; Bouchy, F.] Aix Marseille Univ, CNRS, UMR 7326, LAM, F-13388 Marseille, France.
[Pouzenc, C.] Concordia Stn, Dome C, Japan.
[Valbousquet, F.] Opt Vis, 6 Bis Ave Esterel,BP 69, F-06162 Juan Les Pins, France.
[Barbieri, M.] Univ Atacama, Dept Fis, Copayapu 485, Copiapo, Chile.
[Bouchez, G.] Univ Versailles, GEMAC, CNRS, 45 Ave Etats Unis, F-78035 Versailles, France.
RP Crouzet, N (reprint author), Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM crouzet@dunlap.utoronto.ca
NR 13
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99080U
DI 10.1117/12.2233702
PG 10
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100022
ER
PT S
AU Furesz, G
Simcoe, R
Barnes, SI
Buchhave, LA
Egan, M
Foster, R
Hellickson, T
Malonis, A
Phillips, D
Shectman, S
Walsworth, R
Winn, J
Woods, DF
AF Furesz, Gabor
Simcoe, Robert
Barnes, Stuart I.
Buchhave, Lars A.
Egan, Mark
Foster, Rick
Hellickson, Tim
Malonis, Andrew
Phillips, David
Shectman, Steve
Walsworth, Ronald
Winn, Josh
Woods, Deborah F.
BE Evans, CJ
Simard, L
Takami, H
TI WISDOM: the WIYN Spectrograph for DOppler Monitoring - a NASA-NSF
concept for an extreme precision radial velocity instrument in support
of TESS
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE precision radial velocity spectrograph; white pupil echelle
spectrograph; high resolution spectroscopy; pupil slicer; fiber fed;
near-infrared echelle; EPDS; TESS
AB The Kepler mission highlighted that precision radial velocity (PRV) follow-up is a real bottleneck in supporting transiting exoplanet surveys. The limited availability of PRV instruments, and the desire to break the " 1 m/s" precision barrier, prompted the formation of a NASA-NSF collaboration `NN-EXPLORE' to call for proposals designing a new Extreme Precision Doppler Spectrograph (EPDS). By securing a significant fraction of telescope time on the 3.5m WIYN at Kitt Peak, and aiming for unprecedented long-term precision, the EPDS instrument will provide a unique tool for U.S. astronomers in characterizing exoplanet candidates identified by TESS. One of the two funded instrument concept studies is led by the Massachusetts Institute of Technology, in consortium with Lincoln Laboratories, Harvard-Smithsonian Center for Astrophysics and the Carnegie Observatories. This paper describes the instrument concept WISDOM (WIYN Spectrograph for DOppler Monitoring) prepared by this team.
WISDOM is a fiber fed, environmentally controlled, high resolution (R=110k), asymmetric white-pupil echelle spectrograph, covering a wide 380-1300nm wavelength region. Its R4 and R6 echelle gratings provide the main dispersion, symmetrically mounted on either side of a vertically aligned, vacuum-enclosed carbon fiber optical bench. Each grating feeds two cameras and thus the resulting wavelength range per camera is narrow enough that the VPHG cross-dispersers and employed anti-reflection coatings are highly efficient. The instrument operates near room temperature, and so thermal background for the near-infrared arm is mitigated by thermal blocking filters and a short (1.7 mu m) cutoff HgCdTe detector. To achieve high resolution while maintaining small overall instrument size (100/125mm beam diameter), imposed by the limited available space within the observatory building, we chose to slice the telescope pupil 6 ways before coupling light into fibers. An atmospheric dispersion corrector and fast tip-tilt system assures maximal light gathering within the 1.2 '' entrance aperture. The six octagonal fibers corresponding to each slice of the pupil employ ball-lens double scramblers to stabilize the near-and far-fields. Three apiece are coupled into each of two rectangular fibers, to mitigate modal nose and present a rectilinear illumination pattern at the spectrograph's slit plane. Wavelength solutions are derived from ThAr lamps and an extremely wide coverage dual-channel laser frequency comb. Data is reduced on the fly for evaluation by a custom pipeline, while daily archives and extended scope data reduction products are stored on NExScI servers, also managing archives and access privileges for GTO and GO programs.
C1 [Furesz, Gabor; Simcoe, Robert; Egan, Mark; Foster, Rick; Hellickson, Tim; Malonis, Andrew; Winn, Josh] MIT Kavli Inst Astrophys & Space Res, 77 Mass Ave, Cambridge, MA 02139 USA.
[Barnes, Stuart I.] Stuart Barnes Opt Design, Potsdam, Germany.
[Buchhave, Lars A.] Univ Copenhagen, Copenhagen, Denmark.
[Phillips, David; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Shectman, Steve] Carnegie Observ, Pasadena, CA USA.
[Woods, Deborah F.] MIT Lincoln Lab, Lexington, MA USA.
RP Furesz, G (reprint author), MIT Kavli Inst Astrophys & Space Res, 77 Mass Ave, Cambridge, MA 02139 USA.
EM gfuresz@mit.edu
NR 31
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 990814
DI 10.1117/12.2234376
PG 22
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100030
ER
PT S
AU Jacoby, GH
Bernstein, R
Bouchez, A
Colless, M
Crane, J
Depoy, D
Espeland, B
Hare, T
Jaffe, D
Lawrence, J
Marshall, J
McGregor, P
Shectman, S
Sharp, R
Szentgyorgyi, A
Uomoto, A
Walls, B
AF Jacoby, George H.
Bernstein, R.
Bouchez, A.
Colless, M.
Crane, J.
DePoy, D.
Espeland, B.
Hare, T.
Jaffe, D.
Lawrence, J.
Marshall, J.
McGregor, P.
Shectman, S.
Sharp, R.
Szentgyorgyi, A.
Uomoto, A.
Walls, B.
BE Evans, CJ
Simard, L
Takami, H
TI Instrumentation Progress at the Giant Magellan Telescope Project
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE GMT; ELT; spectrograph; integral-field spectrograph; multi-object
spectrograph; optical instruments; infrared instruments
AB Instrument development for the 24m Giant Magellan Telescope (GMT) is described: current activities, progress, status, and schedule. One instrument team has completed its preliminary design and is currently beginning its final design (GCLEF, an optical 350-950 nm, high-resolution and precision radial velocity echelle spectrograph). A second instrument team is in its conceptual design phase (GMACS, an optical 350-950 nm, medium resolution, 6-10 arcmin field, multi-object spectrograph). A third instrument team is midway through its preliminary design phase (GMTIFS, a near-IR YJHK diffraction-limited imager/integral-field-spectrograph), focused on risk reduction prototyping and design optimization. A fourth instrument team is currently fabricating the 5 silicon immersion gratings needed to begin its preliminary design phase (GMTNIRS, a simultaneous JHKLM high-resolution, AO-fed, echelle spectrograph). And, another instrument team is focusing on technical development and prototyping (MANIFEST, a facility robotic, multifiber- feed, with a 20 arcmin field of view). In addition, a medium-field (6 arcmin, 0.06 arcsec/pix) optical imager will support telescope and AO commissioning activities, and will excel at narrow-band imaging. In the spirit of advancing synergies with other groups, the challenges of running an ELT instrument program and opportunities for cross-ELT collaborations are discussed.
C1 [Jacoby, George H.; Bernstein, R.; Bouchez, A.; Walls, B.] Giant Magellan Telescope Org, 465 N Halstead St, Pasadena, CA 91107 USA.
[Colless, M.; Espeland, B.; McGregor, P.; Sharp, R.] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia.
[Crane, J.; Hare, T.; Shectman, S.; Uomoto, A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[DePoy, D.; Marshall, J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Jaffe, D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Lawrence, J.] Australian Astron Observ, POB 296, Epping, NSW 1710, Australia.
[Szentgyorgyi, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Jacoby, GH (reprint author), Giant Magellan Telescope Org, 465 N Halstead St, Pasadena, CA 91107 USA.
EM gjacoby@gmto.org
OI Colless, Matthew/0000-0001-9552-8075
NR 20
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99081U
DI 10.1117/12.2232809
PG 15
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100049
ER
PT S
AU Lawrence, JS
Ben-Ami, S
Brown, DM
Brown, R
Case, S
Chapman, S
Churilov, V
Colless, M
Content, R
Depoy, D
Evans, I
Farrell, T
Goodwin, M
Jacoby, G
Klauser, U
Kuehn, K
Lorente, NPF
Mali, S
Marshall, JL
Muller, R
Nichani, V
Pai, N
Prochaska, T
Saunders, W
Schmidt, L
Shortridge, K
Staszak, NF
Szentgyorgyi, A
Tims, J
Vuong, M
Waller, L
Zhelem, R
AF Lawrence, Jon S.
Ben-Ami, Sagi
Brown, David M.
Brown, Rebecca
Case, Scott
Chapman, Steve
Churilov, Vladimir
Colless, Matthew
Content, Robert
DePoy, Darren
Evans, Ian
Farrell, Tony
Goodwin, Michael
Jacoby, George
Klauser, Urs
Kuehn, Kyler
Lorente, Nuria P. F.
Mali, Slavko
Marshall, Jennifer L.
Muller, Rolf
Nichani, Vijay
Pai, Naveen
Prochaska, Travis
Saunders, Will
Schmidt, Luke
Shortridge, Keith
Staszak, Nicholas F.
Szentgyorgyi, Andrew
Tims, Julia
Vuong, Minh
Waller, Lew
Zhelem, Ross
BE Evans, CJ
Simard, L
Takami, H
TI The MANIFEST Prototyping Design Study
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE fibre positioner; fibre positioning systems; Starbugs; fibre robots; GMT
AB MANIFEST is a facility multi-object fibre system for the Giant Magellan Telescope, which uses 'Starbug' fibre positioning robots. MANIFEST, when coupled to the telescope's planned seeing-limited instruments, GMACS, and G-CLEF, offers access to: larger fields of view; higher multiplex gains; versatile reformatting of the focal plane via IFUs; image-slicers; and in some cases higher spatial and spectral resolution. The Prototyping Design Study phase for MANIFEST, nearing completion, has focused on developing a working prototype of a Starbugs system, called TAIPAN, for the UK Schmidt Telescope, which will conduct a stellar and galaxy survey of the Southern sky. The Prototyping Design Study has also included work on the GMT instrument interfaces. In this paper, we outline the instrument design features of TAIPAN, highlight the modifications that will be necessary for the MANIFEST implementation, and provide an update on the MANIFEST/instrument interfaces.
C1 [Lawrence, Jon S.; Brown, David M.; Brown, Rebecca; Case, Scott; Chapman, Steve; Churilov, Vladimir; Content, Robert; Farrell, Tony; Goodwin, Michael; Klauser, Urs; Kuehn, Kyler; Lorente, Nuria P. F.; Mali, Slavko; Muller, Rolf; Nichani, Vijay; Pai, Naveen; Saunders, Will; Shortridge, Keith; Staszak, Nicholas F.; Tims, Julia; Vuong, Minh; Waller, Lew; Zhelem, Ross] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Ben-Ami, Sagi; Evans, Ian; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA.
[Colless, Matthew] Australia Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[DePoy, Darren; Marshall, Jennifer L.; Prochaska, Travis; Schmidt, Luke] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Jacoby, George] Giant Magellan Telescope Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
RP Lawrence, JS (reprint author), Australian Astron Observ, N Ryde, NSW 2113, Australia.
EM jl@aao.gov.au
OI Colless, Matthew/0000-0001-9552-8075
NR 30
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99089O
DI 10.1117/12.2232412
PG 15
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100269
ER
PT S
AU Mueller, M
Szentgyorgyi, A
Baldwin, D
Bean, J
Ben-Ami, S
Brennan, P
Budynkiewicz, J
Chun, MY
Crane, JD
Epps, H
Evans, I
Evans, J
Foster, J
Frebel, A
Gauron, T
Glenday, A
Hare, T
Jange, BH
Jang, JG
Jordan, A
Kim, J
Kim, KM
de Oliveira, CM
Mercedes, LM
McCracken, K
McMuldroch, S
Miller, J
Oh, JS
Onyuksel, C
Ordway, M
Park, C
Park, SJ
Paxson, C
Phillips, D
Plummer, D
Podgorski, W
Seifahrt, A
Steiner, J
Uomoto, A
Walsworth, R
Yu, YS
AF Mueller, Mark
Szentgyorgyi, Andrew
Baldwin, Daniel
Bean, Jacob
Ben-Ami, Sagi
Brennan, Patricia
Budynkiewicz, J.
Chun, Moo-Yung
Crane, Jeffrey D.
Epps, Harland
Evans, Ian
Evans, Janet
Foster, Jeff
Frebel, Anna
Gauron, Thomas
Glenday, Alex
Hare, Tyson
Jange, Bi-Ho
Jang, Jeong-Gyun
Jordan, Andres
Kim, Jihun
Kim, Kang-Min
de Oliveira, Claudia Mendes
Mercedes, Lopez-Morales
McCracken, Kenneth
McMuldroch, Stuart
Miller, Joseph
Oh, Jae Sok
Onyuksel, Cem
Ordway, Mark
Park, Chan
Park, Sung-Joon
Paxson, Charles
Phillips, David
Plummer, David
Podgorski, William
Seifahrt, Andreas
Steiner, Joao
Uomoto, Alan
Walsworth, Ronald
Yu, Young-Sam
BE Evans, CJ
Simard, L
Takami, H
TI The Opto-Mechanical Design of the GMT-Consortium Large Earth Finder
(G-CLEF)
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Echelle spectrograph; precision radial velocity; G-CLEF; GMT; optical
mounts; vacuum chamber
AB The GMT-Consortium Large Earth Finder (G-CLEF) is a fiber-fed, optical echelle spectrograph selected as the first light instrument for the Giant Magellan Telescope (GMT) now under construction at the Las Campanas Observatory in Chile. G-CLEF has been designed to be a general-purpose echelle spectrograph with precision radial velocity (PRV) capability for exoplanet detection. The radial velocity (RV) precision goal of G-CLEF is 10 cm/sec, necessary for detection of Earth-sized exoplanets(1). This goal imposes challenging stability requirements on the optical mounts and the overall spectrograph support structures especially when considering the instrument's operational environment. The accuracy of G-CLEF's PRV measurements will be influenced by minute changes in temperature and ambient air pressure as well as vibrations and micro gravity-vector variations caused by normal telescope slewing. For these reasons we have chosen to enclose G-CLEF's spectrograph in a vibration isolated vacuum chamber, within a well-insulated thermal enclosure, at a gravity invariant location on GMT's azimuth platform. Additional design constraints posed by the GMT telescope include: a limited space envelope, a thermal emission ceiling, and a maximum weight allowance. Other factors, such as manufacturability, serviceability, available technology and budget are also significant design drivers. All of the above considerations must be managed while ensuring performance requirements are achieved.
In this paper, we discuss the design of G-CLEF's optical mounts and support structures including the choice of a low coefficient of thermal expansion (CTE) carbon-fiber optical bench to minimize the system's sensitivity to thermal soaks and gradients. We discuss design choices made to the vacuum chamber geared towards minimize the influence of daily ambient pressure variations on image motion during observation. We discuss the design of G-CLEF's insulated enclosure and thermal control systems which will maintain the spectrograph at milli-Kelvin level stability while simultaneously limiting thermal emissions into the telescope dome. Also discussed are micro gravity-vector variations caused by normal telescope slewing, their uncorrected influence on image motion, and how they are dealt with in the design. Finally, we discuss G-CLEF's front-end assembly and fiber-feed system as well as other interface challenges presented by the telescope, enclosure and neighboring instrumentation.
C1 [Mueller, Mark; Szentgyorgyi, Andrew; Baldwin, Daniel; Ben-Ami, Sagi; Brennan, Patricia; Budynkiewicz, J.; Evans, Ian; Evans, Janet; Foster, Jeff; Gauron, Thomas; Glenday, Alex; Mercedes, Lopez-Morales; McCracken, Kenneth; McMuldroch, Stuart; Miller, Joseph; Onyuksel, Cem; Ordway, Mark; Paxson, Charles; Phillips, David; Plummer, David; Podgorski, William; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
[Bean, Jacob; Seifahrt, Andreas; Uomoto, Alan] Univ Chicago, 640 S Ellis Ave, Chicago, IL 60637 USA.
[Crane, Jeffrey D.; Hare, Tyson] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Jordan, Andres] Pontificia Univ Catolica Chile, Vicuna Mackenna 4860, Santiago, Chile.
[Chun, Moo-Yung; Jange, Bi-Ho; Jang, Jeong-Gyun; Kim, Jihun; Kim, Kang-Min; Park, Chan; Park, Sung-Joon; Yu, Young-Sam] Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon, South Korea.
[Frebel, Anna] MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Epps, Harland] Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA.
[de Oliveira, Claudia Mendes; Steiner, Joao] Univ Sao Paulo, Inst Astron Geophys & Atmospher Sci, St Matao 1226, BR-05508090 Sao Paulo, Brazil.
RP Mueller, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 9908A2
DI 10.1117/12.2233246
PG 18
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100280
ER
PT S
AU Oh, JS
Park, C
Kim, J
Kim, KM
Chun, MY
Yu, YS
Lee, S
Nah, J
Park, SJ
Szentgyorgyi, A
McMuldroch, S
Norton, T
Podgorski, W
Evans, I
Mueller, M
Uomoto, A
Crane, J
Hare, T
AF Oh, Jae Sok
Park, Chan
Kim, Jihun
Kim, Kang-Min
Chun, Moo-Young
Yu, Young Sam
Lee, Sungho
Nah, Jakyoung
Park, Sung-Joon
Szentgyorgyi, Andrew
McMuldroch, Stuart
Norton, Timothy
Podgorski, William
Evans, Ian
Mueller, Mark
Uomoto, Alan
Crane, Jeffrey
Hare, Tyson
BE Evans, CJ
Simard, L
Takami, H
TI Optomechanical Design of the G-CLEF Flexure Control Camera System
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE GMT; G-CLEF; GCFEA; FCC; Critical design phase
AB The GMT-Consortium Large Earth Finder (G-CLEF) is the very first light instrument of the Giant Magellan Telescope (GMT). The G-CLEF is a fiber feed, optical band echelle spectrograph that is capable of extremely precise radial velocity measurement. KASI (Korea Astronomy and Space Science Institute) is responsible for Flexure Control Camera (FCC) included in the G-CLEF Front End Assembly (GCFEA). The FCC is a kind of guide camera, which monitors the field images focused on a fiber mirror to control the flexure and the focus errors within the GCFEA. The FCC consists of five optical components: a collimator including triple lenses for producing a pupil, neutral density filters allowing us to use much brighter star as a target or a guide, a tent prism as a focus analyzer for measuring the focus offset at the fiber mirror, a reimaging camera with three pair of lenses for focusing the beam on a CCD focal plane, and a CCD detector for capturing the image on the fiber mirror. In this article, we present the optical and mechanical FCC designs which have been modified after the PDR in April 2015.
C1 [Oh, Jae Sok; Park, Chan; Kim, Jihun; Kim, Kang-Min; Chun, Moo-Young; Yu, Young Sam; Lee, Sungho; Nah, Jakyoung; Park, Sung-Joon] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
[Szentgyorgyi, Andrew; McMuldroch, Stuart; Norton, Timothy; Podgorski, William; Evans, Ian; Mueller, Mark] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
[Uomoto, Alan; Crane, Jeffrey; Hare, Tyson] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
RP Oh, JS (reprint author), Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99089M
DI 10.1117/12.2232147
PG 8
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100267
ER
PT S
AU Quirrenbach, A
Amado, PJ
Caballero, JA
Mundt, R
Reiners, A
Ribas, I
Seifert, W
Abril, M
Aceituno, J
Alonso-Floriano, FJ
Anwand-Heerwart, H
Azzaro, M
Bauer, F
Barrado, D
Becerril, S
Bejar, VJS
Benitez, D
Berdinas, ZM
Brinkmoller, M
Cardenas, MC
Casal, E
Claret, A
Colome, J
Cortes-Contreras, M
Czesla, S
Doellinger, M
Dreizler, S
Feiz, C
Fernandez, M
Ferro, IM
Fuhrmeister, B
Galadi, D
Gallardo, I
Galvez-Ortiz, MC
Garcia-Piquer, A
Garrido, R
Gesa, L
Galera, VG
Hernandez, JIG
Peinado, RG
Grozinger, U
Guardia, J
Guenther, EW
de Guindos, E
Hagen, HJ
Hatzes, AP
Hauschildt, PH
Helmling, J
Henning, T
Hermann, D
Arabi, RH
Castano, LH
Hernando, FH
Herrero, E
Huber, A
Huber, KF
Huke, P
Jeffers, SV
de Juan, E
Kaminski, A
Kehr, M
Kim, M
Klein, R
Kluter, J
Kurster, M
Lafarga, M
Lara, LM
Lamert, A
Laun, W
Launhardt, R
Lemk, U
Lenzen, R
Llamas, M
del Fresno, ML
Lopez-Puertas, M
Lopez-Santiago, J
Salas, JFL
Madinabeitia, HM
Mall, U
Mandel, H
Mancini, L
Molina, JAM
Fernandez, DM
Martin, EL
Martin-Ruiz, S
Marvin, C
Mathar, RJ
Mirabet, E
Montes, D
Morales, JC
Munoz, RM
Nagel, E
Naranjo, V
Nowak, G
Palle, E
Panduro, J
Passegger, VM
Pavlov, A
Pedraz, S
Perez, E
Perez-Medialdea, D
Perger, M
Pluto, M
Ramon, A
Rebolo, R
Redondo, P
Reffert, S
Reinhart, S
Rhode, P
Rix, HW
Rodler, F
Rodriguez, E
Lopez, CR
Rohloff, RR
Rosich, A
Carrasco, MAS
Sanz-Forcada, J
Sarkis, P
Sarmiento, LF
Schafer, S
Schiller, J
Schmidt, C
Schmitt, JHMM
Schofer, P
Schweitzer, A
Shulyak, D
Solano, E
Stahl, O
Storz, C
Tabernero, HM
Tala, M
Tal-Or, L
Ulbrich, RG
Veredas, G
Linares, JIV
Vilardell, F
Wagner, K
Winkler, J
Osorio, MRZ
Zechmeister, M
Ammler-Von Eiff, M
Anglada-Escude, G
del Burgo, C
Garcia-Vargas, ML
Klutsch, A
Lizon, JL
Lopez-Morales, M
Ofir, A
Perez-Calpena, A
Perryman, MAC
Sanchez-Blanco, E
Strachan, JBP
Sturmer, J
Suarez, JC
Trifonov, T
Tulloch, SM
Xu, W
AF Quirrenbach, A.
Amado, P. J.
Caballero, J. A.
Mundt, R.
Reiners, A.
Ribas, I.
Seifert, W.
Abril, M.
Aceituno, J.
Alonso-Floriano, F. J.
Anwand-Heerwart, H.
Azzaro, M.
Bauer, F.
Barrado, D.
Becerril, S.
Bejar, V. J. S.
Benitez, D.
Berdinas, Z. M.
Brinkmoeller, M.
Cardenas, M. C.
Casal, E.
Claret, A.
Colome, J.
Cortes-Contreras, M.
Czesla, S.
Doellinger, M.
Dreizler, S.
Feiz, C.
Fernandez, M.
Ferro, I. M.
Fuhrmeister, B.
Galadi, D.
Gallardo, I.
Galvez-Ortiz, M. C.
Garcia-Piquer, A.
Garrido, R.
Gesa, L.
Gomez Galera, V.
Gonzalez Hernandez, J. I.
Gonzalez Peinado, R.
Groezinger, U.
Guardia, J.
Guenther, E. W.
de Guindos, E.
Hagen, H. -J.
Hatzes, A. P.
Hauschildt, P. H.
Helmling, J.
Henning, T.
Hermann, D.
Hernandez Arabi, R.
Hernandez Castano, L.
Hernandez Hernando, F.
Herrero, E.
Huber, A.
Huber, K. F.
Huke, P.
Jeffers, S. V.
de Juan, E.
Kaminski, A.
Kehr, M.
Kim, M.
Klein, R.
Klueter, J.
Kurster, M.
Lafarga, M.
Lara, L. M.
Lamert, A.
Laun, W.
Launhardt, R.
Lemk, U.
Lenzen, R.
Llamas, M.
Lopez del Fresno, M.
Lopez-Puertas, M.
Lopez-Santiago, J.
Salas, J. F. Lopez
Magan Madinabeitia, H.
Mall, U.
Mandel, H.
Mancini, L.
Marin Molina, J. A.
Maroto Fernandez, D.
Martin, E. L.
Martin-Ruiz, S.
Marvin, C.
Mathar, R. J.
Mirabet, E.
Montes, D.
Morales, J. C.
Morales Munoz, R.
Nagel, E.
Naranjo, V.
Nowak, G.
Palle, E.
Panduro, J.
Passegger, V. M.
Pavlov, A.
Pedraz, S.
Perez, E.
Perez-Medialdea, D.
Perger, M.
Pluto, M.
Ramon, A.
Rebolo, R.
Redondo, P.
Reffert, S.
Reinhart, S.
Rhode, P.
Rix, H. -W.
Rodler, F.
Rodriguez, E.
Rodriguez Lopez, C.
Rohloff, R. -R.
Rosich, A.
Sanchez Carrasco, M. A.
Sanz-Forcada, J.
Sarkis, P.
Sarmiento, L. F.
Schafer, S.
Schiller, J.
Schmidt, C.
Schmitt, J. H. M. M.
Schofer, P.
Schweitzer, A.
Shulyak, D.
Solano, E.
Stahl, O.
Storz, C.
Tabernero, H. M.
Tala, M.
Tal-Or, L.
Ulbrich, R. -G.
Veredas, G.
Vico Linares, J. I.
Vilardell, F.
Wagner, K.
Winkler, J.
Zapatero Osorio, M. R.
Zechmeister, M.
Ammler-von Eiff, M.
Anglada-Escude, G.
del Burgo, C.
Garcia-Vargas, M. L.
Klutsch, A.
Lizon, J. -L.
Lopez-Morales, M.
Ofir, A.
Perez-Calpena, A.
Perryman, M. A. C.
Sanchez-Blanco, E.
Strachan, J. B. P.
Sturmer, J.
Suarez, J. C.
Trifonov, T.
Tulloch, S. M.
Xu, W.
BE Evans, CJ
Simard, L
Takami, H
TI CARMENES: An Overview Six Months After First Light
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Spectrographs; Optical Instrumentation; Near-Infrared Instrumentation;
Extrasolar Planets; M Dwarfs
ID PERFORMANCE; ALGORITHMS; HARPS
AB The CARMENES instrument is a pair of high-resolution (R greater than or similar to 80, 000) spectrographs covering the wavelength range from 0.52 to 1.71 mu m, optimized for precise radial velocity measurements. It was installed and commissioned at the 3.5 m telescope of the Calar Alto observatory in Southern Spain in 2015. The first large science program of CARMENES is a survey of similar to 300 M dwarfs, which started on Jan 1, 2016.
We present an overview of all subsystems of CARMENES (front end, fiber system, visible-light spectrograph, near-infrared spectrograph, calibration units, etalons, facility control, interlock system, instrument control system, data reduction pipeline, data flow, and archive), and give an overview of the assembly, integration, verification, and commissioning phases of the project. We show initial results and discuss further plans for the scientific use of CARMENES.
C1 [Quirrenbach, A.; Caballero, J. A.; Seifert, W.; Brinkmoeller, M.; Feiz, C.; Kaminski, A.; Kim, M.; Klueter, J.; Mandel, H.; Reffert, S.; Stahl, O.; Tala, M.; Veredas, G.; Wagner, K.; Sturmer, J.] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Amado, P. J.; Abril, M.; Becerril, S.; Berdinas, Z. M.; Casal, E.; Claret, A.; Fernandez, M.; Ferro, I. M.; Garrido, R.; Lara, L. M.; Lopez-Puertas, M.; Magan Madinabeitia, H.; Martin-Ruiz, S.; Mirabet, E.; Morales Munoz, R.; Perez, E.; Perez-Medialdea, D.; Ramon, A.; Rodriguez, E.; Rodriguez Lopez, C.; Sanchez Carrasco, M. A.] Inst Astrofis Andalucia CSIC, Glorieta Astron S-N, E-18008 Granada, Spain.
[Caballero, J. A.; Barrado, D.; Galvez-Ortiz, M. C.; Lopez del Fresno, M.; Martin, E. L.; Sanz-Forcada, J.; Solano, E.; Zapatero Osorio, M. R.] Ctr Astrobiol CSIC INTA, Campus ESAC,Camino Bajo Castillo S-N, E-28692 Madrid, Spain.
[Mundt, R.; Cardenas, M. C.; Groezinger, U.; Henning, T.; Hermann, D.; Huber, A.; Klein, R.; Kurster, M.; Laun, W.; Launhardt, R.; Lenzen, R.; Mall, U.; Mancini, L.; Mathar, R. J.; Naranjo, V.; Panduro, J.; Pavlov, A.; Rix, H. -W.; Rodler, F.; Rohloff, R. -R.; Sarkis, P.; Storz, C.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Reiners, A.; Anwand-Heerwart, H.; Bauer, F.; Dreizler, S.; Huke, P.; Jeffers, S. V.; Lamert, A.; Lemk, U.; Marvin, C.; Passegger, V. M.; Rhode, P.; Sarmiento, L. F.; Schafer, S.; Schmidt, C.; Schofer, P.; Shulyak, D.; Tal-Or, L.; Ulbrich, R. -G.; Zechmeister, M.; Ofir, A.] Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
[Ribas, I.; Colome, J.; Garcia-Piquer, A.; Gesa, L.; Guardia, J.; Herrero, E.; Lafarga, M.; Morales, J. C.; Perger, M.; Rosich, A.; Vilardell, F.] Inst Ciencies Espai CSIC IEEC, Campus UAB,C Can Magrans S-N, E-08193 Barcelona, Spain.
[Aceituno, J.; Azzaro, M.; Benitez, D.; Galadi, D.; Gomez Galera, V.; de Guindos, E.; Helmling, J.; Hernandez Arabi, R.; Hernandez Castano, L.; Hernandez Hernando, F.; de Juan, E.; Salas, J. F. Lopez; Marin Molina, J. A.; Maroto Fernandez, D.; Pedraz, S.; Reinhart, S.; Vico Linares, J. I.] Observ Astron Calar Alto, Ctr Astron Hispanoaleman MPG CSIC, E-04550 Gergal, Almeria, Spain.
[Alonso-Floriano, F. J.; Cortes-Contreras, M.; Gallardo, I.; Gonzalez Peinado, R.; Llamas, M.; Lopez-Santiago, J.; Montes, D.; Tabernero, H. M.] Univ Complutense Madrid, Fac Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Bejar, V. J. S.; Gonzalez Hernandez, J. I.; Nowak, G.; Palle, E.; Rebolo, R.; Redondo, P.] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Bejar, V. J. S.; Gonzalez Hernandez, J. I.; Nowak, G.; Palle, E.; Rebolo, R.; Redondo, P.] Univ la Laguna, Dept Astrofis, E-38206 San Cristobal de la Laguna, Tenerife, Spain.
[Czesla, S.; Fuhrmeister, B.; Hagen, H. -J.; Hauschildt, P. H.; Huber, K. F.; Nagel, E.; Schmitt, J. H. M. M.; Schweitzer, A.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Doellinger, M.; Guenther, E. W.; Hatzes, A. P.; Kehr, M.; Pluto, M.; Schiller, J.; Winkler, J.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
[Ammler-von Eiff, M.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Anglada-Escude, G.; Strachan, J. B. P.] Queen Mary Univ London, Sch Phys & Astron, 327 Mile End Rd, London E1 4NS, England.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla 72840, Mexico.
[Garcia-Vargas, M. L.; Perez-Calpena, A.; Tulloch, S. M.] FRACTAL SLNE, C Tulipan 2,P 13,1A, E-28231 Madrid, Spain.
[Klutsch, A.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy.
[Lizon, J. -L.] European Org Astron Res Southern Hemisphere, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Ofir, A.] Weizmann Inst Sci, Dept Earth & Planetary Sci, 234 Herzl St, IL-76100 Rehovot, Israel.
[Perryman, M. A. C.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Sanchez-Blanco, E.] Opt Dev, Ave Pablo Iglesias 7,Local 5, E-41008 Seville, Spain.
[Sturmer, J.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Suarez, J. C.] Univ Granada, Dept Fis Teor & Cosmos, Fuentenueva Campus, E-18007 Granada, Spain.
[Trifonov, T.] Univ Hong Kong, Dept Earth Sci, James Lee Bldg,Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
[Xu, W.] Wenli Xu Opt Syst Engn, Kirchenstr 6, D-74937 Spechbach, Germany.
RP Quirrenbach, A (reprint author), Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany.
EM A.Quirrenbach@lsw.uni-heidelberg.de
OI Vilardell, Francesc/0000-0003-0441-1504; Zapatero Osorio, Maria
Rosa/0000-0001-5664-2852; Anglada Escude, Guillem/0000-0002-3645-5977;
Amado, Pedro Jose/0000-0002-8388-6040; Perez,
Enrique/0000-0001-9737-4559; Barrado, David/0000-0002-5971-9242; Montes,
David/0000-0002-7779-238X
NR 17
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR UNSP 990812
DI 10.1117/12.2231880
PG 14
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100029
ER
PT S
AU Samra, J
Cheimets, P
DeLuca, E
Galeros, J
Gauron, T
Golub, L
Guth, G
Hertz, E
Judge, P
Koutchmy, S
Marquez, V
AF Samra, Jenna
Cheimets, Peter
DeLuca, Edward
Galeros, John
Gauron, Thomas
Golub, Leon
Guth, Giora
Hertz, Edward
Judge, Philip
Koutchmy, Serge
Marquez, Vanessa
BE Evans, CJ
Simard, L
Takami, H
TI An airborne infrared spectrometer for solar eclipse observations
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE AIR-Spec; infrared; spectrometer; solar corona; emission line; magnetic
field; HIAPER; airborne
ID CORONA; LINE
AB This paper presents the design of an innovative solar spectrometer that will fly on the NSF/NCAR Gulfstream V High-Performance Instrumented Airborne Platform for Environmental Research (GV HIAPER) during the 2017 solar eclipse. The airborne infrared spectrometer (AIR-Spec) will search for five infrared coronal emission lines, some of which have never been measured. In addition, it will bring high resolution imaging to GV HIAPER. The instrument development faces the challenges of achieving adequate resolution and signal-to-noise ratio in a compact package mounted to a noisy moving platform. To ensure that AIR-Spec meets its research goals, the instrument is undergoing pre-flight modeling and testing. The results are presented with reference to the instrument requirements.
C1 [Samra, Jenna] Harvard Univ, Cambridge, MA 02138 USA.
[Cheimets, Peter; DeLuca, Edward; Galeros, John; Gauron, Thomas; Golub, Leon; Guth, Giora; Hertz, Edward; Marquez, Vanessa] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Judge, Philip] NCAR High Altitude Observ, Boulder, CO USA.
[Koutchmy, Serge] Inst Astrophys Paris, Paris, France.
RP Samra, J (reprint author), Harvard Univ, Cambridge, MA 02138 USA.
FU National Science Foundation Major Research Instrumentation (NSF)
[AGS-1531549]
FX National Science Foundation Major Research Instrumentation grant, NSF
AGS-1531549: Development of an Airborne Infrared Spectrometer (AIR-Spec)
to Enable Coronal Emission Line Observations During the 2017 Great
American Solar Eclipse.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99085U
DI 10.1117/12.2232128
PG 13
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100165
ER
PT S
AU Siverd, RJ
Brown, TM
Hygelund, J
Henderson, T
Tufts, JR
Eastman, JD
van Eyken, J
Barnes, S
AF Siverd, Robert J.
Brown, Timothy M.
Hygelund, John.
Henderson, Todd
Tufts, Joseph R.
Eastman, Jason D.
van Eyken, Julian
Barnes, Stuart
BE Evans, CJ
Simard, L
Takami, H
TI NRES: the Network of Robotic Echelle Spectrographs
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE LCOGT; NRES; echelle; fiber; exoplanet spectrograph; radial velocity;
robotic
ID TELESCOPE
AB Las Cumbres Observatory Global Network (LCOGT) is building the Network of Robotic Echelle Spectrographs (NRES), which will consist of six identical, optical (390 - 860 nm) high-precision spectrographs, each fiber-fed simultaneously by up to two 1-meter telescopes and a thorium argon calibration source. We plan to install one at up to 6 observatory sites in the Northern and Southern hemispheres, creating a single, globally-distributed, autonomous spectrograph facility using up to twelve 1-meter telescopes. Simulations suggest we will achieve long-term radial velocity precision of 3 m/s in less than an hour for stars brighter than V = 12. We have been funded with NSF MRI and ATI grants, and expect our first spectrograph to be deployed in fall 2016, with the full network operation of 5 or 6 units beginning in 2017. We will briefly overview the NRES design, goals, robotic operation, and status. In addition, we will discuss early results from our prototype spectrograph, the laboratory and on-sky performance of our first production unit, and the ongoing software development effort to bring this resource online.
C1 [Siverd, Robert J.; Brown, Timothy M.; Hygelund, John.; Henderson, Todd; Tufts, Joseph R.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Ste 102, Goleta, CA 93117 USA.
[Eastman, Jason D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van Eyken, Julian] CALTECH, NASA, Exoplanet Sci Inst, 770 South Wilson Ave,M-S 100-22, Pasadena, CA 91125 USA.
[Barnes, Stuart] Stuart Barnes Opt Design, NL-1094 NK Amsterdam, Netherlands.
RP Siverd, RJ (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Ste 102, Goleta, CA 93117 USA.
EM rsiverd@lcogt.net
FU National Science Foundation (NSF) [AST-1229720, AST-1508464]
FX Funding for the NRES spectrographs was provided through MRI Grant
AST-1229720 and ATI grant AST-1508464 from the National Science
Foundation (NSF). We are grateful for their ongoing support.
NR 8
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 99086X
DI 10.1117/12.2233188
PG 7
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100194
ER
PT S
AU Szentgyorgyi, A
Baldwin, D
Barnes, S
Bean, J
Ben-Ami, S
Brennan, P
Budynkiewicz, J
Chun, MY
Conroy, C
Crane, JD
Epps, H
Evans, I
Evans, J
Foster, J
Frebel, A
Gauron, T
Guzman, D
Hare, T
Jang, BH
Jang, JG
Jordan, A
Kim, J
Kim, KM
de Oliveira, CM
Lopez-Morales, M
McCracken, K
McMuldroch, S
Miller, J
Mueller, M
Oh, JS
Onyuksel, C
Ordway, M
Park, BG
Park, C
Park, SJ
Paxson, C
Phillips, D
Plummer, D
Podgorski, W
Seifahrt, A
Stark, D
Steiner, J
Uomoto, A
Walsworth, R
Yu, YS
AF Szentgyorgyi, Andrew
Baldwin, Daniel
Barnes, Stuart
Bean, Jacob
Ben-Ami, Sagi
Brennan, Patricia
Budynkiewicz, Jamie
Chun, Moo-Yung
Conroy, Charlie
Crane, Jeffrey D.
Epps, Harland
Evans, Ian
Evans, Janet
Foster, Jeff
Frebel, Anna
Gauron, Thomas
Guzman, Dani
Hare, Tyson
Jang, Bi-Ho
Jang, Jeong-Gyun
Jordan, Andres
Kim, Jihun
Kim, Kang-Min
de Oliveira, Claudia Mendes
Lopez-Morales, Mercedes
McCracken, Kenneth
McMuldroch, Stuart
Miller, Joseph
Mueller, Mark
Oh, Jae Sok
Onyuksel, Cem
Ordway, Mark
Park, Byeong-Gon
Park, Chan
Park, Sung-Joon
Paxson, Charles
Phillips, David
Plummer, David
Podgorski, William
Seifahrt, Andreas
Stark, Daniel
Steiner, Joao
Uomoto, Alan
Walsworth, Ronald
Yu, Young-Sam
BE Evans, CJ
Simard, L
Takami, H
TI The GMT-Consortium Large Earth Finder (G-CLEF): An optical echelle
spectrograph for the Giant Magellan Telescope (GMT)
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Echelle spectrograph; precision radial velocity; G-CLEF; GMT; high
dispersion spectroscopy; ELTs
ID SPECTROSCOPY
AB The GMT-Consortium Large Earth Finder (G-CLEF) will be a cross-dispersed, optical band echelle spectrograph to be delivered as the first light scientific instrument for the Giant Magellan Telescope (GMT) in 2022. G-CLEF is vacuumenclosed and fiber-fed to enable precision radial velocity (PRV) measurements, especially for the detection and characterization of low-mass exoplanets orbiting solar-type stars. The passband of G-CLEF is broad, extending from 3500 angstrom to . This passband provides good sensitivity at blue wavelengths for stellar abundance studies and deep red response for observations of high-redshift phenomena. The design of G-CLEF incorporates several novel technical innovations. We give an overview of the innovative features of the current design. G-CLEF will be the first PRV spectrograph to have a composite optical bench so as to exploit that material's extremely low coefficient of thermal expansion, high in-plane thermal conductivity and high stiffness-to-mass ratio. The spectrograph camera subsystem is divided into a red and a blue channel, split by a dichroic, so there are two independent refractive spectrograph cameras. The control system software is being developed in model-driven software context that has been adopted globally by the GMT. G-CLEF has been conceived and designed within a strict systems engineering framework. As a part of this process, we have developed a analytical toolset to assess the predicted performance of G-CLEF as it has evolved through design phases.
C1 [Szentgyorgyi, Andrew; Baldwin, Daniel; Barnes, Stuart; Ben-Ami, Sagi; Brennan, Patricia; Budynkiewicz, Jamie; Conroy, Charlie; Evans, Ian; Evans, Janet; Foster, Jeff; Gauron, Thomas; Lopez-Morales, Mercedes; McCracken, Kenneth; McMuldroch, Stuart; Miller, Joseph; Mueller, Mark; Onyuksel, Cem; Ordway, Mark; Paxson, Charles; Phillips, David; Plummer, David; Podgorski, William; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
[Stark, Daniel] Univ Arizona, Steward Observ, 933 North Cherry St, Tucson, AZ 85721 USA.
[Crane, Jeffrey D.; Hare, Tyson; Uomoto, Alan] Carnegie Inst Sci, The Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Guzman, Dani; Kim, Jihun] Pontificia Univ Catolica Chile, Vicuna Mackenna 4860, Santiago, Chile.
[Bean, Jacob; Seifahrt, Andreas] Univ Chicago, 640 S Ellis Ave, Chicago, IL 60637 USA.
[Chun, Moo-Yung; Jang, Bi-Ho; Jang, Jeong-Gyun; Jordan, Andres; Kim, Kang-Min; Park, Byeong-Gon; Park, Chan; Park, Sung-Joon] Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon, South Korea.
[Frebel, Anna] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Epps, Harland] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[de Oliveira, Claudia Mendes; Steiner, Joao] Univ Sao Paulo, Rua Matao 1226, BR-05508900 Sao Paulo, Brazil.
RP Szentgyorgyi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
NR 32
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 990822
DI 10.1117/12.2233506
PG 19
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100057
ER
PT S
AU Wang, SY
Ling, HH
Hu, YS
Geary, JC
Chang, YC
Chen, HY
Amato, SM
Huang, PJ
Pratlong, J
Szentgyorgyi, A
Lehner, M
Norton, T
Jorden, P
AF Wang, Shiang-Yu
Ling, Hung-Hsu
Hu, Yen-Sang
Geary, John C.
Chang, Yin-Chang
Chen, Hsin-Yo
Amato, Stephen M.
Huang, Pin-Jie
Pratlong, Jerome
Szentgyorgyi, Andrew
Lehner, Matthew
Norton, Timothy
Jorden, Paul
BE Evans, CJ
Simard, L
Takami, H
TI The Prototype Cameras for Transneptunian Automatic Occultation Survey
SO GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Instrumentation for Astronomy VI
CY JUN 26-30, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Camera; CMOS sensor; high speed; mosaic; photometry
AB The Transneptunian Automated Occultation Survey (TAOS II) is a three robotic telescope project to detect the stellar occultation events generated by TransNeptunian Objects (TNOs). TAOS II project aims to monitor about 10000 stars simultaneously at 20Hz to enable statistically significant event rate. The TAOS II camera is designed to cover the 1.7 degrees diameter field of view of the 1.3m telescope with 10 mosaic 4.5kx2k CMOS sensors. The new CMOS sensor (CIS 113) has a back illumination thinned structure and high sensitivity to provide similar performance to that of the back-illumination thinned CCDs. Due to the requirements of high performance and high speed, the development of the new CMOS sensor is still in progress. Before the science arrays are delivered, a prototype camera is developed to help on the commissioning of the robotic telescope system. The prototype camera uses the small format e2v CIS 107 device but with the same dewar and also the similar control electronics as the TAOS II science camera. The sensors, mounted on a single Invar plate, are cooled to the operation temperature of about 200K as the science array by a cryogenic cooler. The Invar plate is connected to the dewar body through a supporting ring with three G10 bipods. The control electronics consists of analog part and a Xilinx FPGA based digital circuit. One FPGA is needed to control and process the signal from a CMOS sensor for 20Hz region of interests (ROI) readout.
C1 [Wang, Shiang-Yu; Ling, Hung-Hsu; Hu, Yen-Sang; Chang, Yin-Chang; Chen, Hsin-Yo; Huang, Pin-Jie; Lehner, Matthew] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei, Taiwan.
[Geary, John C.; Amato, Stephen M.; Szentgyorgyi, Andrew; Norton, Timothy] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Pratlong, Jerome; Jorden, Paul] e2v, Waterhouse Lane, Chelmsford CM1 2QU, Essex, England.
RP Wang, SY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei, Taiwan.
EM sywang@asiaa.sinica.edu.tw
NR 7
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0196-3
J9 PROC SPIE
PY 2016
VL 9908
AR 990846
DI 10.1117/12.2232062
PG 6
WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics
GA BG7NF
UT WOS:000391509100121
ER
PT J
AU White, ND
Barrowclough, GF
Groth, JG
Braun, MJ
AF White, Noor D.
Barrowclough, George F.
Groth, Jeff G.
Braun, Michael J.
TI A MULTI-GENE ESTIMATE OF HIGHER-LEVEL PHYLOGENETIC RELATIONSHIPS AMONG
NIGHTJARS (AVES: CAPRIMULGIDAE)
SO ORNITOLOGIA NEOTROPICAL
LA English
DT Article
DE Caprimulgidae; Molecular phylogeny; Nightjars; Partitioning; Strisores
ID AVIAN ORDER CAPRIMULGIFORMES; COALESCENT MODEL; ULTRACONSERVED ELEMENTS;
BIRDS; PHYLOGENOMICS; ALLIES; TREE; TIMESCALES; SELECTION; MARKERS
AB The higher-level phylogenetic relationships of the nightjars and nighthawks (Caprimulgidae) have been challenging for traditional systematics due to their cryptic plumage and conservative morphology. We explored these relationships by combining two previously published molecular datasets with new data to generate a complete matrix (7,104 bp) of evolutionarily disparate sequence elements from four genes for 36 taxa. We analyzed each of the genes separately for base composition heterogeneity and heterozygosity. We analyzed the concatenated matrix in a likelihood framework using seven different partitioning schemes. As the number of subsets in a given partitioning scheme increased, tree length and likelihood score also increased; however, the branching topology was little affected by increasingly complex partitioning schemes. Our best maximum likelihood tree has increased bootstrap support at 13 of 30 ingroup nodes compared with previous analyses, a result likely due to doubling the length of the sequence data. Coalescent-based species tree inference produced a tree congruent with all strongly supported nodes in the maximum likelihood tree. This topology agrees with previous molecular studies in identifying three small, early branching Old World genera (Eurostopodus, Lyncornis, and Gactornis) and four more speciose terminal clades, representing the New World nighthawks (genus Chordeiles) and three nightjar radiations centered in South America, Central America and the Old World, respectively. Increased node support across the tree reinforces a historical scenario with origins in the region surrounding the Indian Ocean, followed by diversification in the New World and subsequent recolonization and radiation in the Old World. Future work on this group should incorporate additional members of the genera Lyncornis and Eurostopodus, to determine which is the basal lineage of Caprimulgidae.
C1 [White, Noor D.; Braun, Michael J.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.
[White, Noor D.; Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
[Barrowclough, George F.; Groth, Jeff G.] Amer Museum Nat Hist, Dept Ornithol, Cent Pk West 79th St, New York, NY 10024 USA.
RP White, ND (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.; White, ND (reprint author), Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
EM noordwhite@gmail.com
FU Scholarly Studies Program; Consortium for Understanding and Sustaining a
Biodiverse Planet
FX We thank Matthew Kweskin for technical assistance on computational
analyses, Laura Kubatko for discussion of SVDquartets, and David L.
Swofford and Robert Lanfear for discussion of issues related to
partitioning. We thank Charles Mitter for constructive comments on an
early draft of this manuscript, Minh Le for assistance with some of the
RAG-1 sequencing for this project, Thiago V. V. da Costa for sharing his
unpublished dissertation, and Natalia Agudelo and Gustavo S. Cabanne for
translating the abstract. NDW received Smithsonian Institution support
from the Scholarly Studies Program, from the Consortium for
Understanding and Sustaining a Biodiverse Planet, and as a Predoctoral
Fellow. Computations in this paper were run on the Smithsonian
Institution's High Performance Cluster.
NR 50
TC 0
Z9 0
U1 1
U2 1
PU NEOTROPICAL ORNITHOLOGICAL SOC, USGS PATUXENT WILDLIFE RESEARCH CTR
PI ATHENS
PA UNIV GEORGIA, WARNELL SCH FOREST RESOURCES, ATHENS, GA 30602-2152 USA
SN 1075-4377
J9 ORNITOL NEOTROP
JI ORNITOL. NEOTROP.
PY 2016
VL 27
BP 223
EP 236
PG 14
WC Ornithology
SC Zoology
GA EI1XK
UT WOS:000392279800001
ER
PT S
AU Marseglia, L
Saha, K
Ajoy, A
Schroder, T
Englund, D
Teraji, T
Isoya, J
Jelezko, F
Walsworth, R
Pacheco, JL
Perry, DL
Bielejec, ES
Cappellaro, P
AF Marseglia, L.
Saha, K.
Ajoy, A.
Schroder, T.
Englund, D.
Teraji, T.
Isoya, J.
Jelezko, F.
Walsworth, R.
Pacheco, J. L.
Perry, D. L.
Bielejec, E. S.
Cappellaro, P.
GP IEEE
TI A bright nanowire single photon source
SO 2016 CONFERENCE ON LASERS AND ELECTRO-OPTICS (CLEO)
SE Conference on Lasers and Electro-Optics
LA English
DT Proceedings Paper
CT Conference on Lasers and Electro-Optics (CLEO)
CY JUN 05-10, 2016
CL San Jose, CA
AB Silicon-vacancy ( SiV) centers in diamond are bright sources of indistinguishable single photons. We report fabrication of nanowires coupled to single SiV by deterministic ion implantation, yielding greatly enhanced light coupling compared to SiV in bulk.
C1 [Marseglia, L.; Saha, K.; Ajoy, A.; Schroder, T.; Englund, D.; Cappellaro, P.] MIT, Elect Res Lab, Cambridge, MA 02139 USA.
[Teraji, T.] NIMS, Tsukuba, Ibaraki 3050047, Japan.
[Isoya, J.] Univ Tsukuba, Tsukuba, Ibaraki 3058571, Japan.
[Marseglia, L.; Jelezko, F.] Univ Ulm, D-89081 Ulm, Germany.
[Walsworth, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pacheco, J. L.; Perry, D. L.; Bielejec, E. S.] Sandia Labs, Albuquerque, NM 87123 USA.
RP Marseglia, L (reprint author), MIT, Elect Res Lab, Cambridge, MA 02139 USA.; Marseglia, L (reprint author), Univ Ulm, D-89081 Ulm, Germany.
EM lucamars@mit.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2160-9020
BN 978-1-9435-8011-8
J9 CONF LASER ELECTR
PY 2016
PG 2
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA BG7HE
UT WOS:000391286401061
ER
PT J
AU Tagliabue, G
Borgini, A
Tittarelli, A
van Donkelaar, A
Martin, RV
Bertoldi, M
Fabiano, S
Maghini, A
Codazzi, T
Scaburri, A
Favia, I
Cau, A
Barigelletti, G
Tessandori, R
Contiero, P
AF Tagliabue, Giovanna
Borgini, Alessandro
Tittarelli, Andrea
van Donkelaar, Aaron
Martin, Randall V.
Bertoldi, Martina
Fabiano, Sabrina
Maghini, Anna
Codazzi, Tiziana
Scaburri, Alessandra
Favia, Imma
Cau, Alessandro
Barigelletti, Giulio
Tessandori, Roberto
Contiero, Paolo
TI Atmospheric fine particulate matter and breast cancer mortality: a
population-based cohort study
SO BMJ OPEN
LA English
DT Article
ID AIR-POLLUTION; EXPOSURE; HEALTH; RISK; LIFE; NUTRITION; IMPACT; WOMEN
AB Objectives: Atmospheric fine particulate matter (PM2.5) has multiple adverse effects on human health. Global atmospheric levels of PM2.5 increased by 0.55 mu g/m(3)/year (2.1%/year) from 1998 through 2012. There is evidence of a causal relationship between atmospheric PM2.5 and breast cancer (BC) incidence, but few studies have investigated BC mortality and atmospheric PM2.5. We investigated BC mortality in relation to atmospheric PM2.5 levels among patients living in Varese Province, northern Italy.
Methods: We selected female BC cases, archived in the local population-based cancer registry, diagnosed at age 50-69 years, between 2003 and 2009. The geographic coordinates of each woman's place of residence were identified, and individual PM2.5 exposures were assessed from satellite data. Grade, stage, age at diagnosis, period of diagnosis and participation in BC screening were potential confounders. Kaplan-Meir and Nelson-Aalen methods were used to test for mortality differences in relation to PM2.5 quartiles. Multivariable Cox proportional hazards modelling estimated HRs and 95% CIs of BC death in relation to PM2.5 exposure.
Results: Of 2021 BC cases, 325 died during follow-up to 31 December 2013, 246 for BC. Risk of BC death was significantly higher for all three upper quartiles of PM2.5 exposure compared to the lowest, with HRs of death: 1.82 (95% CI 1.15 to 2.89), 1.73 (95% CI 1.12 to 2.67) and 1.72 (95% CI 1.08 to 2.75).
Conclusions: Our study indicates that the risk of BC mortality increases with PM2.5 exposure. Although additional research is required to confirm these findings, they are further evidence that PM2.5 exposure is harmful and indicate an urgent need to improve global air quality.
C1 [Tagliabue, Giovanna; Tittarelli, Andrea; Fabiano, Sabrina; Maghini, Anna; Codazzi, Tiziana; Barigelletti, Giulio] Fdn IRCCS Ist Nazl Tumori, Canc Registry Unit, Milan, Italy.
[Borgini, Alessandro; Bertoldi, Martina; Scaburri, Alessandra; Favia, Imma; Cau, Alessandro; Contiero, Paolo] Fdn IRCCS Ist Nazl Tumori, Environm Epidemiol Unit, Milan, Italy.
[van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Tessandori, Roberto] Prov Sondrio, Local Hlth Unit, Sondrio, Italy.
RP Contiero, P (reprint author), Fdn IRCCS Ist Nazl Tumori, Environm Epidemiol Unit, Milan, Italy.
EM paolo.contiero@istitutotumori.mi.it
RI Borgini, Alessandro/D-2980-2017; Tittarelli, Andrea/D-3008-2017;
Tagliabue, Giovanna /D-4194-2017; Contiero, Paolo/F-6721-2016
OI Borgini, Alessandro/0000-0002-5167-4297; Tittarelli,
Andrea/0000-0002-8865-5129; Tagliabue, Giovanna /0000-0001-8165-5524;
Contiero, Paolo/0000-0001-6760-3605
NR 27
TC 0
Z9 0
U1 2
U2 2
PU BMJ PUBLISHING GROUP
PI LONDON
PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND
SN 2044-6055
J9 BMJ OPEN
JI BMJ Open
PY 2016
VL 6
IS 11
AR e012580
DI 10.1136/bmjopen-2016-012580
PG 6
WC Medicine, General & Internal
SC General & Internal Medicine
GA EG8JQ
UT WOS:000391303400188
PM 28076275
ER
PT J
AU Greenwalt, DE
Moulton, JK
AF Greenwalt, Dale E.
Moulton, John K.
TI The first fossil New World Dixidae with a critical discussion of generic
definitions
SO PALAEONTOLOGIA ELECTRONICA
LA English
DT Article
DE Dixidae; Eocene insect fossil; Kishenehn Formation; venation; new
species
ID TRUE FLIES INSECTA; DIPTERA DIXIDAE; FAMILIES; NEMATOCERA; PHYLOGENY;
EVOLUTION; THAILAND; KOREA; LIFE; DYAR
AB Four new fossil species of the dipteran family Dixidae, including the first fossil specimens of females in this family, are described from the Middle Eocene Kishenehn Formation oil shales of northwestern Montana. These new species, Dixella intacta sp. nov., D. eomarginata sp. nov., D. spinilobata sp. nov. and D. curvistyla sp. nov., are the first fossils of Dixidae to be described from the New World. The morphological bases of all generic assignments of extant and extinct dixids are critically reviewed, and new data on wing venation pattern variability in extant Dixidae are presented. It is concluded that it is impossible to distinguish between adults of the two major genera, Dixa and Dixella, based solely on wing venation. Given the lack of distinguishing features, the names of the two Cenozoic species that consist only of a single wing, Dixa priscula and D. cimbrica, are declared nomina dubia and the fossils are assigned to Dixidae incertae sedis.
C1 [Greenwalt, Dale E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,10th & Constitut Ave NW, Washington, DC 20013 USA.
[Moulton, John K.] Univ Tennessee, Entomol & Plant Pathol Dept, 432 Biotechnol Bldg,2505 EJ Chapman Dr, Knoxville, TN 37996 USA.
RP Greenwalt, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,10th & Constitut Ave NW, Washington, DC 20013 USA.
EM GreenwaltD@si.edu; jmoulton@utk.edu
FU Dept. of Paleobiology, NMNH
FX We thank C. Labandeira (Dept. of Paleobiology, NMNH) for sponsorship and
administrative support and F. Marsh (Dept. of Paleobiology, NMNH) for
his ongoing assistance. We also thank J. Pecor of the Walter Reed
Biosystematics unit located in the Smithsonian Institution's MSC in
Suitland, MD, and C. Mellish of the Earth Sciences Department of the
NHM, London for access to specimens. We also wish to thank an anonymous
reviewer and A. Borkent and S. Brady for numerous and insightful
comments that led to significant improvements in the manuscript. This is
contribution number 277 of the Evolution of Terrestrial Ecosystems
Consortium of the National Museum of Natural History in Washington, D.C.
NR 88
TC 0
Z9 0
U1 1
U2 1
PU COQUINA PRESS
PI AMHERST
PA C/O WHITEY HAGADORN, EXECUTIVE EDITOR, AMHERST COLLEGE, DEPT GEOLOGY,
AMHERST, MA 01002 USA
SN 1935-3952
EI 1094-8074
J9 PALAEONTOL ELECTRON
JI Palaeontol. electron.
PY 2016
VL 19
IS 3
AR 55A
PG 32
WC Paleontology
SC Paleontology
GA EH9PD
UT WOS:000392102400016
ER
PT J
AU Turner, BL
Bielnicka, AW
Dalling, JW
Wolf, JA
AF Turner, Benjamin L.
Bielnicka, Aleksandra W.
Dalling, James W.
Wolf, Jeffrey A.
TI Interference by Iron in the Determination of Boron by ICP-OES in
Mehlich-III Extracts and Total Element Digests of Tropical Forest Soils
SO COMMUNICATIONS IN SOIL SCIENCE AND PLANT ANALYSIS
LA English
DT Article
DE Boron; CaCl2-extraction; ICP-OES; Mehlich-III extraction; total element
digestion; tropical forests
ID EL-NINO; SPECIES DISTRIBUTIONS; ORGANIC PHOSPHORUS; NUTRIENTS; DYNAMICS;
GRADIENT; DROUGHT; PLANTS
AB Boron detection in soil extracts by inductively-coupled plasma optical-emission spectrometry (ICP-OES) can be influenced by iron interference, particularly in strongly weathered tropical forest soils. Boron concentrations in Mehlich-III extracts of 230 soils under lowland tropical forest in Panama were markedly overestimated at the most sensitive ICP-OES wavelength (249.772 nm) compared to a less sensitive but interference-free wavelength (208.957 nm) due to iron interference. Hot-water extracts contained insufficient iron to interfere in boron detection, but boron quantification in total element digests was affected strongly by iron interference at 249.772 nm. The relationship between boron overestimation and iron was used to correct a database of 300 Mehlich-III extractable boron measurements made at 249.772 nm for soils from a large forest dynamics plot. We recommend that boron measurements in tropical forest soils by ICP-OES should use the less sensitive 208.957 nm wavelength to avoid interference by extracted iron.
C1 [Turner, Benjamin L.; Bielnicka, Aleksandra W.; Dalling, James W.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL USA.
[Wolf, Jeffrey A.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM TurnerBL@si.edu
NR 31
TC 0
Z9 0
U1 3
U2 3
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0010-3624
EI 1532-2416
J9 COMMUN SOIL SCI PLAN
JI Commun. Soil Sci. Plant Anal.
PY 2016
VL 47
IS 21
BP 2378
EP 2386
DI 10.1080/00103624.2016.1228952
PG 9
WC Agronomy; Plant Sciences; Chemistry, Analytical; Soil Science
SC Agriculture; Plant Sciences; Chemistry
GA EF9QW
UT WOS:000390665700002
ER
PT S
AU Baez, GP
Rogers, C
Labrada, JER
AF Baez, Gabriela Perez
Rogers, Chris
Labrada, Jorge Emilio Roses
BE Baez, GP
Rogers, C
Labrada, JER
TI Introduction
SO LANGUAGE DOCUMENTATION AND REVITALIZATION IN LATIN AMERICAN CONTEXTS
SE Trends in Linguistics-Studies and Monographs
LA English
DT Proceedings Paper
CT 87th Annual Meeting of the Linguistic-Society-of-America
CY JAN 03-06, 2013
CL Boston, MA
SP Linguist Soc Amer
ID LANGUAGES
C1 [Baez, Gabriela Perez] Smithsonian Inst, Washington, DC 20560 USA.
[Rogers, Chris] Brigham Young Univ, Provo, UT 84602 USA.
[Labrada, Jorge Emilio Roses] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
RP Baez, GP (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 68
TC 0
Z9 0
U1 0
U2 0
PU DE GRUYTER MOUTON
PI BERLIN 11
PA GENTHINER STR 13, POSTF 110240, W-1000 BERLIN 11, GERMANY
SN 1861-4302
BN 978-3-11-042890-2; 978-3-11-043807-9
J9 TRENDS LINGUIST-STUD
PY 2016
VL 295
BP 1
EP 28
PG 28
WC Linguistics; Language & Linguistics
SC Linguistics
GA BG6SQ
UT WOS:000390839900001
ER
PT S
AU Baez, GP
AF Baez, Gabriela Perez
BE Baez, GP
Rogers, C
Labrada, JER
TI Addressing the gap between community beliefs and priorities and
researchers' language maintenance interests
SO LANGUAGE DOCUMENTATION AND REVITALIZATION IN LATIN AMERICAN CONTEXTS
SE Trends in Linguistics-Studies and Monographs
LA English
DT Proceedings Paper
CT 87th Annual Meeting of the Linguistic-Society-of-America
CY JAN 03-06, 2013
CL Boston, MA
SP Linguist Soc Amer
C1 [Baez, Gabriela Perez] Smithsonian Inst, Washington, DC 20560 USA.
RP Baez, GP (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 47
TC 0
Z9 0
U1 0
U2 0
PU DE GRUYTER MOUTON
PI BERLIN 11
PA GENTHINER STR 13, POSTF 110240, W-1000 BERLIN 11, GERMANY
SN 1861-4302
BN 978-3-11-042890-2; 978-3-11-043807-9
J9 TRENDS LINGUIST-STUD
PY 2016
VL 295
BP 165
EP 194
PG 30
WC Linguistics; Language & Linguistics
SC Linguistics
GA BG6SQ
UT WOS:000390839900007
ER
PT S
AU Allured, R
Hertz, E
Marquez, V
Cotroneo, V
Wallace, M
Salmaso, B
Civitani, MM
Trolier-McKinstry, S
Vikhlinin, AA
Pareschi, G
Reid, PB
AF Allured, Ryan
Hertz, Edward
Marquez, Vanessa
Cotroneo, Vincenzo
Wallace, Margeaux
Salmaso, Bianca
Civitani, Marta M.
Trolier-McKinstry, Susan
Vikhlinin, Alexey A.
Pareschi, Giovanni
Reid, Paul B.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Laboratory Demonstration of the Piezoelectric Figure Control of a
Cylindrical Slumped Glass Optic
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray optics; X-ray Surveyor; Adjustable Optics; X-ray Astronomy
AB The X-ray Surveyor is a mission concept for a next generation X-ray observatory. This mission will feature roughly 30 times the effective area of the Chandra Observatory while matching its sub-arcsecond angular resolution. The key to meeting these requirements is lightweight, segmented optics. To ensure these optics achieve and maintain sub-arcsecond performance, we propose to use piezoelectric coatings for post-bonding and on-orbit figure correction. We have fabricated a cylindrical prototype optic with piezoelectric adjusters and measured its performance using optical metrology. We present the results of this experiment and discuss their implications for an observatory featuring adjustable X-ray optics.
C1 [Allured, Ryan; Hertz, Edward; Marquez, Vanessa; Cotroneo, Vincenzo; Vikhlinin, Alexey A.; Reid, Paul B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Wallace, Margeaux; Trolier-McKinstry, Susan] Penn State Univ, University Pk, PA 16802 USA.
[Salmaso, Bianca; Civitani, Marta M.; Pareschi, Giovanni] Osserv Astron Brera, Brera, Italy.
RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990554-1
DI 10.1117/12.2233827
PN 1
PG 8
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500145
ER
PT S
AU Allured, R
McEntaffer, RL
Hertz, E
Cheimets, PN
Smith, RK
AF Allured, Ryan
McEntaffer, Randall L.
Hertz, Edward
Cheimets, Peter N.
Smith, Randall K.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Optical design considerations and raytracing results for the Arcus
grating spectrometer concept
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Arcus; X-ray spectroscopy; X-ray optics; silicon pore optics; off plane
reflection gratings
AB Arcus is a mission concept for a next generation X-ray grating spectrometer. It will offer spectral resolution (lambda/Delta lambda) greater than 2000 combined with over 500 cm(2) of effective area in the 2.1-2.4 nm bandpass. These capabilities will elucidate the cycle of baryonic matter in and out of galaxies, the means by which supermassive black holes influence their surroundings, and the early formation and evolution of solar systems. We present the overall optical design of the mission, which features four arrays of silicon pore optics modules with four matching arrays of off-plane reflection grating modules. These optics disperse the incident X-rays over the 12 m focal length in four separate conical diffraction patterns onto CCD arrays at the focal plane. Each array of optics is an azimuthal sub-aperture of the typical Wolter telescope design, enabling enhanced spectral resolution due to an asymmetric point spread function. The theoretical spectral resolution, effective area, and alignment tolerances have been determined via raytrace modeling.
C1 [Allured, Ryan; Hertz, Edward; Cheimets, Peter N.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[McEntaffer, Randall L.] Penn State Univ, University Pk, PA 16802 USA.
RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 15
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99054O
DI 10.1117/12.2233763
PN 1
PG 9
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500135
ER
PT S
AU Arenberg, J
Alluree, R
Reid, P
AF Arenberg, Jonathan
Alluree, Ryan
Reid, Paul
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI A Performance Budget for the X-ray Surveyor Telescope
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray Surveyor; Error Budget; Active Optics
AB This paper uses an budgeting approach to examine the proposed X-ray Surveyor's imaging quality. The paper presents a budget which is the same structure as that of the Chandra X-ray Observatory. The budget is populated with terms that can be expected to be the same as that of Chandra, namely the contributions due to aspect solution and alignment between the mirrors and focal plane detectors. An allocation for dynamic induced image degradation is then introduced, to allow for contribution due to the optics from all sources to be determined, (similar to)0.44 arcseconds. This value is compared with the current state of the art, which is considerably in excess of 0.5 arcesconds. The role and possibility of adjustable optics for the X-ray Surveyor is discussed.
C1 [Arenberg, Jonathan] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA.
[Alluree, Ryan; Reid, Paul] Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Arenberg, J (reprint author), Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA.
NR 11
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990555-1
DI 10.1117/12.2234495
PN 1
PG 7
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500146
ER
PT S
AU Bandler, SR
Adams, JS
Chervenak, JA
Datesman, AM
Eckart, ME
Finkbeiner, FM
Kelley, RL
Kilbourne, CA
Betancourt-Martineza, G
Miniussi, AR
Porter, FS
Sadleir, JE
Sakai, K
Smith, SJ
Stevenson, TR
Wakeham, NA
Wassell, EJ
Yoon, W
Becker, D
Bennett, D
Doriese, WB
Fowler, JW
Gard, JD
Hilton, GC
Mates, B
Morgan, KM
Reintsema, CD
Swetz, D
Ullom, JN
Chaudhuri, S
Irwin, KD
Lee, SJ
Vikhlinin, A
AF Bandler, Simon R.
Adams, Joseph S.
Chervenak, James A.
Datesman, Aaron M.
Eckart, Megan E.
Finkbeiner, Fred M.
Kelley, Richard L.
Kilbourne, Caroline A.
Betancourt-Martineza, Gabriel
Miniussi, Antoine R.
Porter, Frederick S.
Sadleir, John E.
Sakai, Kazuhiro
Smith, Stephen J.
Stevenson, Thomas R.
Wakeham, Nicholas A.
Wassell, Edward J.
Yoon, Wonsik
Becker, Dan
Bennett, Douglas
Doriese, Wilham B.
Fowler, Joseph W.
Gard, Johnathon D.
Hilton, Gene C.
Mates, Benjamin
Morgan, Kelsey M.
Reintsema, Carl D.
Swetz, Daniel
Ullom, Joel N.
Chaudhuri, Saptarshi
Irwin, Kent D.
Lee, Sang-Jun
Vikhlinin, Alexey
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Development of x-ray microcalorimeter imaging spectrometers for the
X-ray Surveyor mission concept
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray Surveyor; microcalorimeter; hydra; multiplexing
ID METALLIC MAGNETIC CALORIMETERS; TRANSITION-EDGE SENSORS; MULTIPLEXER
AB Four astrophysics missions are currently being studied by NASA as candidate large missions to be chosen in the 2020 astrophysics decadal survey.(1) One of these missions is the "X-Ray Surveyor" (XRS), and possible configurations of this mission are currently under study by a science and technology definition team (STDT). One of the key instruments under study is an X-ray microcalorimeter, and the requirements for such an instrument are currently under discussion. In this paper we review some different detector options that exist for this instrument, and discuss what array formats might be possible. We have developed one design option that utilizes either transition-edge sensor (TES) or magnetically coupled calorimeters (MCC) in pixel array-sizes approaching 100 kilo-pixels. To reduce the number of sensors read out to a plausible scale, we have assumed detector geometries in which a thermal sensor such a TES or MCC can read out a sub-array of 20-25 individual 1" pixels. In this paper we describe the development status of these detectors, and also discuss the different options that exist for reading out the very large number of pixels.
C1 [Bandler, Simon R.; Adams, Joseph S.; Chervenak, James A.; Datesman, Aaron M.; Eckart, Megan E.; Finkbeiner, Fred M.; Kelley, Richard L.; Kilbourne, Caroline A.; Betancourt-Martineza, Gabriel; Miniussi, Antoine R.; Porter, Frederick S.; Sadleir, John E.; Sakai, Kazuhiro; Smith, Stephen J.; Stevenson, Thomas R.; Wakeham, Nicholas A.; Wassell, Edward J.; Yoon, Wonsik] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Adams, Joseph S.; Smith, Stephen J.] CRESST, Baltimore, MD 21250 USA.
[Adams, Joseph S.; Smith, Stephen J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Betancourt-Martineza, Gabriel] CRESST, College Pk, MD 20742 USA.
[Betancourt-Martineza, Gabriel] Univ Maryland Coll Pk, College Pk, MD 20742 USA.
[Miniussi, Antoine R.; Sakai, Kazuhiro] CRESST, Greenbelt, MD 20771 USA.
[Miniussi, Antoine R.; Sakai, Kazuhiro] Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Wakeham, Nicholas A.; Yoon, Wonsik] Univ Space Res Assoc, NASA Postdoctoral Program, Greenbelt, MD 20771 USA.
[Finkbeiner, Fred M.] Wyle Informat Syst Inc, Mclean, VA 22102 USA.
[Datesman, Aaron M.; Wassell, Edward J.] Stinger Ghaffarian Technol, Greenbelt, MD 20771 USA.
[Becker, Dan; Bennett, Douglas; Doriese, Wilham B.; Fowler, Joseph W.; Gard, Johnathon D.; Hilton, Gene C.; Mates, Benjamin; Morgan, Kelsey M.; Reintsema, Carl D.; Swetz, Daniel; Ullom, Joel N.] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Gard, Johnathon D.; Mates, Benjamin; Ullom, Joel N.] Univ Colorado, Boulder, CO 80309 USA.
[Chaudhuri, Saptarshi; Irwin, Kent D.; Lee, Sang-Jun] Stanford Univ, Palo Alto, CA 94305 USA.
[Vikhlinin, Alexey] Smithsonian Astrophys Observ, Cambridge, MA 02912 USA.
RP Bandler, SR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Simon.R.Bandler@nasa.gov
NR 37
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99050Q
DI 10.1117/12.2232156
PN 1
PG 12
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500017
ER
PT S
AU Brenneman, LW
Smith, RK
Bregman, J
Kaastra, J
Brickhouse, N
Allured, R
Foster, A
Wolk, S
Wilms, J
Valencic, L
Willingale, R
Grant, C
Bautz, M
Heilmann, R
Huenemoerder, D
Miller, E
Nowak, M
Schattenburg, M
Schulz, N
Burwitz, V
Nandra, K
Sanders, J
Bookbinder, J
Petre, R
Ptak, A
Smale, A
Burrows, D
Poppenhager, K
Costantini, E
Deroo, C
McEntaffer, R
Mushotzky, R
Miller, JM
Temi, P
AF Brenneman, Laura W.
Smith, Randall K.
Bregman, J.
Kaastra, J.
Brickhouse, N.
Allured, R.
Foster, A.
Wolk, S.
Wilms, J.
Valencic, L.
Willingale, R.
Grant, C.
Bautz, M.
Heilmann, R.
Huenemoerder, D.
Miller, E.
Nowak, M.
Schattenburg, M.
Schulz, N.
Burwitz, V.
Nandra, K.
Sanders, J.
Bookbinder, J.
Petre, R.
Ptak, A.
Smale, A.
Burrows, D.
Poppenhager, K.
Costantini, E.
DeRoo, C.
McEntaffer, R.
Mushotzky, R.
Miller, J. M.
Temi, P.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI The evolution of structure and feedback with Arcus
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Large-scale structure; Active galaxies; Stars; Accretion; Outflows;
X-rays; Spectroscopy; Gratings
ID X-RAY SPECTROSCOPY; HOT GASEOUS HALO; T-TAURI STARS;
INTERSTELLAR-MEDIUM; MULTIWAVELENGTH CAMPAIGN; GALAXY CLUSTERS;
XMM-NEWTON; STELLAR WIND; BLACK-HOLE; GAS HALO
AB Arcus is a NASA/MIDEX mission under development in response to the anticipated 2016 call for proposals. It is a free-flying, soft X-ray grating spectrometer with the highest-ever spectral resolution in the 8-51 angstrom (0.24 - 1.55 keV) energy range. The Arcus bandpass includes the most sensitive tracers of diffuse million-degree gas: spectral lines from O VII and O VIII, H- and He-like lines of C, N, Ne and Mg, and unique density-and temperature-sensitive lines from Si and Fe ions. These capabilities enable an advance in our understanding of the formation and evolution of baryons in the Universe that is unachievable with any other present or planned observatory. The mission will address multiple key questions posed in the Decadal Survey(1) and NASA's 2013 Roadmap(2): How do baryons cycle in and out of galaxies? How do black holes and stars influence their surroundings and the cosmic web via feedback? How do stars, circumstellar disks and exoplanet atmospheres form and evolve? Arcus data will answer these questions by leveraging recent developments in off-plane gratings and silicon pore optics to measure X-ray spectra at high resolution from a wide range of sources within and beyond the Milky Way. CCDs with strong Suzaku heritage combined with electronics based on the Swift mission will detect the dispersed X-rays. Arcus will support a broad astrophysical research program, and its superior resolution and sensitivity in soft X-rays will complement the forthcoming Athena calorimeter, which will have comparably high resolution above 2 keV.
C1 [Brenneman, Laura W.; Smith, Randall K.; Brickhouse, N.; Allured, R.; Foster, A.; Wolk, S.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Bregman, J.; Miller, J. M.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
[Kaastra, J.; Costantini, E.] SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Wilms, J.; Petre, R.; Ptak, A.; Smale, A.] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, Sternwartstr 7, D-96049 Bamberg, Germany.
[Valencic, L.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr Phys & Astron, Room 366,3400 N Charles St, Baltimore, MD 21218 USA.
[Valencic, L.] NASA GSFC, Code 662, Greenbelt, MD 20771 USA.
[Willingale, R.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
[Grant, C.; Bautz, M.; Heilmann, R.; Huenemoerder, D.; Miller, E.; Nowak, M.; Schattenburg, M.; Schulz, N.] MIT, 70 Vassar Str,Bldg 37,NE80-6075, Cambridge, MA 02139 USA.
[Burwitz, V.; Nandra, K.; Sanders, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Bookbinder, J.; Temi, P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Burrows, D.] Penn State Univ, Dept Astron & Astrophys, 517 Davey Lab, University Pk, PA 16802 USA.
[Poppenhager, K.] Queens Univ Belfast, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
[DeRoo, C.; McEntaffer, R.] Univ Iowa, Dept Phys & Astron, 203 Van Allen Hall, Iowa City, IA 52242 USA.
[Mushotzky, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Brenneman, LW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM lbrenneman@cfa.harvard.edu
NR 78
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99054P
DI 10.1117/12.2231193
PN 1
PG 18
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500136
ER
PT S
AU Burrows, DN
Hughes, E
Anderson, T
Falcone, AD
Reichard, K
Bautz, M
Kraft, R
AF Burrows, David N.
Hughes, Eli
Anderson, Tyler
Falcone, Abraham D.
Reichard, Karl
Bautz, Mark
Kraft, Ralph
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Fast event recognition for X-ray silicon imagers
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE instrumentation: X-rays; instrumentation: readout electronics;
instrumentation: miscellaneous; space vehicles: instruments
ID DETECTORS; ASTRONOMY
AB Future X-ray astronomy observatories will employ high-speed silicon-based active pixel sensors to obtain wide fields of view with good radiation hardness and low levels of detector saturation (pileup). Detector readout rates envisioned for missions such as Athena and X-ray Surveyor are far too high for existing software-based event recognition techniques to be able to extract the X-ray events from the data stream. We report on the development of high-speed event recognition electronics tailored to the requirements of these new detectors.
C1 [Burrows, David N.; Hughes, Eli; Anderson, Tyler; Falcone, Abraham D.; Reichard, Karl] Penn State Univ, University Pk, PA 16802 USA.
[Bautz, Mark] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Kraft, Ralph] Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Burrows, DN (reprint author), Penn State Univ, University Pk, PA 16802 USA.
EM burrows@astro.psu.edu
NR 10
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99050L
DI 10.1117/12.2231005
PN 1
PG 13
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500014
ER
PT S
AU Champey, P
Winebarger, A
Kobayashi, K
Savage, S
Cirtain, J
Cheimets, P
Hertz, E
Golub, L
Ramsey, B
McCracken, J
Marquez, V
Allured, R
Heilmann, RK
Schattenburg, M
Bruccoleri, A
AF Champey, Patrick
Winebarger, Amy
Kobayashi, Ken
Savage, Sabrina
Cirtain, Jonathan
Cheimets, Peter
Hertz, Edward
Golub, Leon
Ramsey, Brian
McCracken, Jeff
Marquez, Vanessa
Allured, Ryan
Heilmann, Ralf K.
Schattenburg, Mark
Bruccoleri, Alexander
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI On the Alignment and Focusing of the Marshall Grazing Incidence X-ray
Spectrometer (MaGIXS)
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray; Alignment; Sounding Rocket
AB The Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) is a NASA sounding rocket instrument that is designed to observe soft X-ray emissions from 24 - 6.0 angstrom (0.5 - 2.0 keV energies) in the solar atmosphere. For the first time, high-temperature, low-emission plasma will be observed directly with 5 arcsecond spatial resolution and 22 m angstrom spectral resolution. The unique optical design consists of a Wolter - I telescope and a 3-optic grazing-incidence spectrometer. The spectrometer utilizes a finite conjugate mirror pair and a blazed planar, varied line spaced grating, which is directly printed on a silicon substrate using e-beam lithography. The grating design is being finalized and the grating will be fabricated by the Massachusetts Institute of Technology (MIT) and Izentis LLC. Marshall Space Flight Center (MSFC) is producing the nickel replicated telescope and spectrometer mirrors using the same facilities and techniques as those developed for the ART-XC and FOXSI mirrors. The Smithsonian Astrophysical Observatory (SAO) will mount and align the optical sub-assemblies based on previous experience with similar instruments, such as the Hinode X-Ray Telescope (XRT). The telescope and spectrometer assembly will be aligned in visible light through the implementation of a theodolite and reference mirrors, in addition to the centroid detector assembly (CDA) a device designed to align the AXAF-I nested mirrors. Focusing of the telescope and spectrometer will be achieved using the X-ray source in the Stray Light Facility (SLF) at MSFC. We present results from an alignment sensitivity analysis performed on the on the system and we also discuss the method for aligning and focusing MaGIXS.
C1 [Champey, Patrick] Univ Alabama, Huntsville, AL 35899 USA.
[Champey, Patrick; Winebarger, Amy; Kobayashi, Ken; Savage, Sabrina; Cirtain, Jonathan; Ramsey, Brian; McCracken, Jeff] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Cheimets, Peter; Hertz, Edward; Golub, Leon; Marquez, Vanessa; Allured, Ryan] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Heilmann, Ralf K.; Schattenburg, Mark] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Bruccoleri, Alexander] Izentis LLC, Cambridge, MA USA.
RP Champey, P (reprint author), Univ Alabama, Huntsville, AL 35899 USA.; Champey, P (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM patrick.r.champey@nasa.gov
RI Heilmann, Ralf/D-4680-2009
NR 11
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990573
DI 10.1117/12.2232820
PN 1
PG 12
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500195
ER
PT S
AU Feroci, M
Bozzo, E
Brandt, S
Hernanz, M
van der Klis, M
Liu, LP
Orleanski, P
Pohl, M
Santangelo, A
Schanne, S
Stella, L
Takahashi, T
Tamura, H
Watts, A
Wilms, J
Zane, S
Zhang, SN
Bhattacharyya, S
Agudo, I
Ahangarianabhari, M
Albertus, C
Alford, M
Alpar, A
Altamirano, D
Alvarez, L
Amati, L
Amoros, C
Andersson, N
Antonelli, A
Argan, A
Artigue, R
Artigues, B
Atteia, JL
Azzarello, P
Bakala, P
Ballantyne, DR
Baldazzi, G
Baldo, M
Balman, S
Barbera, M
van Baren, C
Barret, D
Baykal, A
Begelman, M
Behar, E
Behar, O
Belloni, T
Bellutti, P
Bernardini, F
Bertuccio, G
Bianchi, S
Bianchini, A
Binko, P
Blay, P
Bocchino, F
Bode, M
Bodin, P
Bombaci, I
Bidaud, JMB
Borghi, G
Boutloukos, S
Bouyjou, F
Bradley, L
Braga, J
Briggs, MS
Brown, E
Buballa, M
Bucciantini, N
Burderi, L
Burgay, M
Bursa, M
Budtz-Jorgensen, C
Cackett, E
Cadoux, FR
Cais, P
Caliandro, GA
Campana, R
Campana, S
Cao, X
Capitanio, F
Casares, J
Casella, P
Castro-Tirado, AJ
Cavazzutim, E
Cavechi, Y
Celestin, S
Cerda-Duran, P
Chakrabarty, D
Chamel, N
Chateau, F
Chen, C
Chen, Y
Chen, Y
Chenevez, J
Chernyakova, M
Coker, J
Cole, R
Collura, A
Coriat, M
Cornelisse, R
Costamante, L
Cros, A
Cui, W
Cumming, A
Cusumano, G
Czerny, B
D'Ai, A
D'Ammando, F
D'Elia, V
Dai, Z
Del Monte, E
De Luca, A
De Martino, D
Dercksen, JPC
De Pasquale, M
De Rosa, A
Del Santo, M
Di Cosimol, S
Degenaar, N
den Herder, JW
Diebold, S
Di Salvo, T
Dong, Y
Donnarumma, I
Doroshenko, V
Doyle, G
Drake, SA
Durant, M
Emmanoulopoulos, D
Enoto, T
Erkut, MH
Esposito, P
Evangelista, Y
Fabian, A
Falanga, M
Favre, Y
Feldman, C
Fender, R
Peng, H
Evangelista, V
Ferrigno, C
Ficorella, F
Finger, M
Finger, MH
Fraser, GW
Frericks, M
Fullekrug, M
Fuschino, F
Gabler, M
Galloway, DK
Sanchez, JLG
Gandhi, P
Gao, Z
Garcia-Berro, E
Gendre, B
Gevin, O
Gezari, S
Giles, AB
Gilfanov, M
Giommi, P
Giovannini, G
Giroletti, M
Gogus, E
Goldwurm, A
Goluchova, K
Gotz, D
Gou, L
Gouiffes, C
Grandi, P
Grassi, M
Greiner, J
Grinberg, V
Groot, P
Gschwender, M
Gualtieri, L
Guedel, M
Guidorzi, C
Guy, L
Haas, D
Haensel, P
Hailey, M
Hamuguchi, K
Hansen, F
Hartmann, DH
Haswell, CA
Hebeler, K
Heger, A
Hempel, M
Hermsen, W
Homan, J
Hornstrup, A
Hudec, R
Huovelin, J
Huppenkothen, D
Inam, SC
Ingram, A
in't Zand, JJM
Israel, G
Iwasawa, K
Izzo, L
Jacobs, HM
Jetter, F
Johannsen, T
Jacobs, HM
Jenke, PA
Jonker, P
Jose, J
Kaaret, P
Kalamkar, M
Kalemci, E
Kanbach, G
Karas, V
Karelin, D
Kataria, D
Keek, L
Kennedy, T
Klochkov, D
Kluzniak, W
Koerding, E
Kokkotas, K
Komossa, S
Korpela, S
Kouveliotou, C
Kowalski, AF
Kreykenbohm, I
Kuiper, LM
Kunneriath, D
Kurkela, A
Kuvvetli, I
La Franca, F
Labanti, C
Lai, D
Lamb, FK
Lachaud, C
Laubert, PP
Lebrun, F
Li, X
Liang, E
Limousin, O
Lin, D
Linares, M
Lodato, G
Lodato, G
Longo, F
Lu, F
Lund, N
Maccarone, TJ
Macera, D
Maestre, S
Mahmoodifar, S
Maier, D
Malcovati, P
Malzac, J
Malone, C
Mandel, I
Mangano, V
Manousakis, A
Marelli, JM
Margueron, J
Marisaldi, M
Markoff, SB
Markowitz, A
Marinucci, A
Martindale, A
Martinez, G
McHardy, IM
Medina-Tanco, G
Mehdipour, M
Melatos, A
Mendez, M
Mereghetti, S
Migliari, S
Mignani, R
Michalska, M
Mihara, T
Miller, MC
Miller, JM
Mineo, T
Miniuttill, G
Morsink, S
Motch, C
Motta, S
Mouchet, M
Mouret, G
Mulacova, J
Muleri, F
Munoz-Darias, T
Negueruela, I
Neilsen, J
Neubert, T
Norton, AJ
Nowak, M
Nucita, A
O'Brien, P
Oertel, M
Olsen, PEH
Orienti, M
Orio, M
Orlandini, M
Osborne, JP
Osten, R
Ozel, F
Pacciani, L
Paerels, F
Paltani, S
Paolillo, M
Papadakis, I
Papitto, A
Paragi, Z
Paredes, JM
Patruno, A
Paul, B
Pederiva, F
Perinati, E
Pellizzoni, A
Penacchioni, AV
Peretz, U
Perez, MA
Perez-Torres, M
Peterson, BM
Petracek, V
Picciotto, A
Piemonte, C
Pittoril, C
Pons, J
Portell, J
Possenti, A
Postnov, K
Poutanen, J
Prakash, M
Prandoni, I
Le Provost, H
Psaltis, D
Pye, J
Qu, J
Rambaud, D
Ramon, P
Ramsay, G
Rapisarda, M
Rachevski, A
Rashevskaya, I
Ray, PS
Rea, N
Reddy, S
Reig, P
Aranda, MR
Remillard, R
Reynolds, C
Rezzolla, L
Ribo, M
de la Rie, R
Riggio, A
Rios, A
Rischke, DH
Rodriguez-Gil, P
Rodriguez, J
Rohlfs, R
Romano, P
Rossi, EMR
Rozanska, A
Rousseau, A
Rudak, B
Russell, DM
Ryde, F
Sabau-Graziati, L
Sakamoto, T
Sala, G
Salvaterra, R
Salvetti, D
Sanna, A
Sandberg, J
Savolainen, T
Scaringi, S
Schaffner-Bielich, J
Schatz, H
Schee, J
Schmid, C
Serino, M
Shakura, N
Shore, S
Schnittman, JD
Schneider, R
Schwenk, A
Schwope, AD
Sedrakian, A
Seyler, JY
Shearer, A
Slowikowska, A
Sims, M
Smith, A
Smith, DM
Smith, PJ
Sobolewska, M
Sochora, V
Soffitta, P
Soleri, P
Song, L
Spencer, A
Stamerra, A
Stappers, B
Staubert, R
Steiner, AW
Stergioulas, N
Stevens, AL
Stratta, G
Strohmayer, TE
Stuchlik, Z
Suchy, S
Suleimanovi, V
Tamburini, F
Tauris, T
Tavecchio, F
Tenzer, C
Thielemann, FK
Tiengo, A
Tolos, L
Tombesi, F
Tomsick, J
Torok, G
Torrejon, JM
Torres, DF
Torresi, E
Tramacere, A
Traulsen, I
Trois, A
Turolla, R
Turriziani, S
Type, S
Uter, P
Uttley, P
Vacchi, A
Varniere, P
Vaughan, S
Vercellone, S
Vietri, M
Vincent, FH
Vrba, V
Walton, D
Wang, J
Wang, Z
Watanabe, S
Wawrzaszek, R
Webb, N
Weinberg, N
Wende, H
Wheatley, P
Wijers, R
Wijnands, R
Wille, M
Wilson-Hodge, CA
Winter, B
Walk, SJ
Wood, K
Woosley, SE
Wu, X
Xiao, L
Xu, R
Yu, W
Yuan, F
Yuan, W
Yuan, Y
Zampa, G
Zampa, N
Zampieri, L
Zdunik, L
Zdziarski, A
Zech, A
Zhang, B
Zhang, C
Zhang, S
Zingale, M
Zorzi, N
Zwart, F
AF Feroci, M.
Bozzo, E.
Brandt, S.
Hernanz, M.
van der Klis, M.
Liu, L. -P.
Orleanski, P.
Pohl, M.
Santangelo, A.
Schanne, S.
Stella, L.
Takahashi, T.
Tamura, H.
Watts, A.
Wilms, J.
Zane, S.
Zhang, S. -N.
Bhattacharyya, S.
Agudo, I.
Ahangarianabhari, M.
Albertus, C.
Alford, M.
Alpar, A.
Altamirano, D.
Alvarez, L.
Amati, L.
Amoros, C.
Andersson, N.
Antonelli, A.
Argan, A.
Artigue, R.
Artigues, B.
Atteia, J. -L.
Azzarello, P.
Bakala, P.
Ballantyne, D. R.
Baldazzi, G.
Baldo, M.
Balman, S.
Barbera, M.
van Baren, C.
Barret, D.
Baykal, A.
Begelman, M.
Behar, E.
Behar, O.
Belloni, T.
Bellutti, P.
Bernardini, F.
Bertuccio, G.
Bianchi, S.
Bianchini, A.
Binko, P.
Blay, P.
Bocchino, F.
Bode, M.
Bodin, P.
Bombaci, I.
Bidaud, J. -M. Bonnet
Borghi, G.
Boutloukos, S.
Bouyjou, F.
Bradley, L.
Braga, J.
Briggs, M. S.
Brown, E.
Buballa, M.
Bucciantini, N.
Burderi, L.
Burgay, M.
Bursa, M.
Budtz-Jorgensen, C.
Cackett, E.
Cadoux, F. R.
Cais, P.
Caliandro, G. A.
Campana, R.
Campana, S.
Cao, X.
Capitanio, F.
Casares, J.
Casella, P.
Castro-Tirado, A. J.
Cavazzutim, E.
Cavechi, Y.
Celestin, S.
Cerda-Duran, P.
Chakrabarty, D.
Chamel, N.
Chateau, F.
Chen, C.
Chen, Y.
Chen, Y.
Chenevez, J.
Chernyakova, M.
Coker, J.
Cole, R.
Collura, A.
Coriat, M.
Cornelisse, R.
Costamante, L.
Cros, A.
Cui, W.
Cumming, A.
Cusumano, G.
Czerny, B.
D'Ai, A.
D'Ammando, F.
D'Elia, V.
Dai, Z.
Del Monte, E.
De Luca, A.
De Martino, D.
Dercksen, J. P. C.
De Pasquale, M.
De Rosa, A.
Del Santo, M.
Di Cosimol, S.
Degenaar, N.
den Herder, J. W.
Diebold, S.
Di Salvo, T.
Dong, Y.
Donnarumma, I.
Doroshenko, V.
Doyle, G.
Drake, S. A.
Durant, M.
Emmanoulopoulos, D.
Enoto, T.
Erkut, M. H.
Esposito, P.
Evangelista, Y.
Fabian, A.
Falanga, M.
Favre, Y.
Feldman, C.
Fender, R.
Peng, H.
Evangelista, V.
Ferrigno, C.
Ficorella, F.
Finger, M.
Finger, M. H.
Fraser, G. W.
Frericks, M.
Fullekrug, M.
Fuschino, F.
Gabler, M.
Galloway, D. K.
Galvez Sanchez, J. L.
Gandhi, P.
Gao, Z.
Garcia-Berro, E.
Gendre, B.
Gevin, O.
Gezari, S.
Giles, A. B.
Gilfanov, M.
Giommi, P.
Giovannini, G.
Giroletti, M.
Gogus, E.
Goldwurm, A.
Goluchova, K.
Gotz, D.
Gou, L.
Gouiffes, C.
Grandi, P.
Grassi, M.
Greiner, J.
Grinberg, V.
Groot, P.
Gschwender, M.
Gualtieri, L.
Guedel, M.
Guidorzi, C.
Guy, L.
Haas, D.
Haensel, P.
Hailey, M.
Hamuguchi, K.
Hansen, F.
Hartmann, D. H.
Haswell, C. A.
Hebeler, K.
Heger, A.
Hempel, M.
Hermsen, W.
Homan, J.
Hornstrup, A.
Hudec, R.
Huovelin, J.
Huppenkothen, D.
Inam, S. C.
Ingram, A.
in't Zand, J. J. M.
Israel, G.
Iwasawa, K.
Izzo, L.
Jacobs, H. M.
Jetter, F.
Johannsen, T.
Jacobs, H. M.
Jenke, P. A.
Jonker, P.
Jose, J.
Kaaret, P.
Kalamkar, M.
Kalemci, E.
Kanbach, G.
Karas, V.
Karelin, D.
Kataria, D.
Keek, L.
Kennedy, T.
Klochkov, D.
Kluzniak, W.
Koerding, E.
Kokkotas, K.
Komossa, S.
Korpela, S.
Kouveliotou, C.
Kowalski, A. F.
Kreykenbohm, I.
Kuiper, L. M.
Kunneriath, D.
Kurkela, A.
Kuvvetli, I.
La Franca, F.
Labanti, C.
Lai, D.
Lamb, F. K.
Lachaud, C.
Laubert, P. P.
Lebrun, F.
Li, X.
Liang, E.
Limousin, O.
Lin, D.
Linares, M.
Lodato, G.
Lodato, G.
Longo, F.
Lu, F.
Lund, N.
Maccarone, T. J.
Macera, D.
Maestre, S.
Mahmoodifar, S.
Maier, D.
Malcovati, P.
Malzac, J.
Malone, C.
Mandel, I.
Mangano, V.
Manousakis, A.
Marelli, J. MargueronM.
Margueron, J.
Marisaldi, M.
Markoff, S. B.
Markowitz, A.
Marinucci, A.
Martindale, A.
Martinez, G.
McHardy, I. M.
Medina-Tanco, G.
Mehdipour, M.
Melatos, A.
Mendez, M.
Mereghetti, S.
Migliari, S.
Mignani, R.
Michalska, M.
Mihara, T.
Miller, M. C.
Miller, J. M.
Mineo, T.
Miniuttill, G.
Morsink, S.
Motch, C.
Motta, S.
Mouchet, M.
Mouret, G.
Mulacova, J.
Muleri, F.
Munoz-Darias, T.
Negueruela, I.
Neilsen, J.
Neubert, T.
Norton, A. J.
Nowak, M.
Nucita, A.
O'Brien, P.
Oertel, M.
Olsen, P. E. H.
Orienti, M.
Orio, M.
Orlandini, M.
Osborne, J. P.
Osten, R.
Ozel, F.
Pacciani, L.
Paerels, F.
Paltani, S.
Paolillo, M.
Papadakis, I.
Papitto, A.
Paragi, Z.
Paredes, J. M.
Patruno, A.
Paul, B.
Pederiva, F.
Perinati, E.
Pellizzoni, A.
Penacchioni, A. V.
Peretz, U.
Perez, M. A.
Perez-Torres, M.
Peterson, B. M.
Petracek, V.
Picciotto, A.
Piemonte, C.
Pittoril, C.
Pons, J.
Portell, J.
Possenti, A.
Postnov, K.
Poutanen, J.
Prakash, M.
Prandoni, I.
Le Provost, H.
Psaltis, D.
Pye, J.
Qu, J.
Rambaud, D.
Ramon, P.
Ramsay, G.
Rapisarda, M.
Rachevski, A.
Rashevskaya, I.
Ray, P. S.
Rea, N.
Reddy, S.
Reig, P.
Reina Aranda, M.
Remillard, R.
Reynolds, C.
Rezzolla, L.
Ribo, M.
de la Rie, R.
Riggio, A.
Rios, A.
Rischke, D. H.
Rodriguez-Gil, P.
Rodriguez, J.
Rohlfs, R.
Romano, P.
Rossi, E. M. R.
Rozanska, A.
Rousseau, A.
Rudak, B.
Russell, D. M.
Ryde, F.
Sabau-Graziati, L.
Sakamoto, T.
Sala, G.
Salvaterra, R.
Salvetti, D.
Sanna, A.
Sandberg, J.
Savolainen, T.
Scaringi, S.
Schaffner-Bielich, J.
Schatz, H.
Schee, J.
Schmid, C.
Serino, M.
Shakura, N.
Shore, S.
Schnittman, J. D.
Schneider, R.
Schwenk, A.
Schwope, A. D.
Sedrakian, A.
Seyler, J. -Y.
Shearer, A.
Slowikowska, A.
Sims, M.
Smith, A.
Smith, D. M.
Smith, P. J.
Sobolewska, M.
Sochora, V.
Soffitta, P.
Soleri, P.
Song, L.
Spencer, A.
Stamerra, A.
Stappers, B.
Staubert, R.
Steiner, A. W.
Stergioulas, N.
Stevens, A. L.
Stratta, G.
Strohmayer, T. E.
Stuchlik, Z.
Suchy, S.
Suleimanovi, V.
Tamburini, F.
Tauris, T.
Tavecchio, F.
Tenzer, C.
Thielemann, F. K.
Tiengo, A.
Tolos, L.
Tombesi, F.
Tomsick, J.
Torok, G.
Torrejon, J. M.
Torres, D. F.
Torresi, E.
Tramacere, A.
Traulsen, I.
Trois, A.
Turolla, R.
Turriziani, S.
Type, S.
Uter, P.
Uttley, P.
Vacchi, A.
Varniere, P.
Vaughan, S.
Vercellone, S.
Vietri, M.
Vincent, F. H.
Vrba, V.
Walton, D.
Wang, J.
Wang, Z.
Watanabe, S.
Wawrzaszek, R.
Webb, N.
Weinberg, N.
Wende, H.
Wheatley, P.
Wijers, R.
Wijnands, R.
Wille, M.
Wilson-Hodge, C. A.
Winter, B.
Walk, S. J.
Wood, K.
Woosley, S. E.
Wu, X.
Xiao, L.
Xu, R.
Yu, W.
Yuan, F.
Yuan, W.
Yuan, Y.
Zampa, G.
Zampa, N.
Zampieri, L.
Zdunik, L.
Zdziarski, A.
Zech, A.
Zhang, B.
Zhang, C.
Zhang, S.
Zingale, M.
Zorzi, N.
Zwart, F.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI The LOFT mission concept - A status update
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray astronomy; Silicon detectors; timing; spectroscopy
AB The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, > 8m(2) effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e. g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission.
C1 [Feroci, M.; Argan, A.; Campana, R.; Capitanio, F.; Del Monte, E.; De Rosa, A.; Del Santo, M.; Di Cosimol, S.; Donnarumma, I.; Evangelista, Y.; Iwasawa, K.; Muleri, F.; Pacciani, L.; Rapisarda, M.; Soffitta, P.; Trois, A.] IAPS INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
[Feroci, M.; Campana, R.; Evangelista, Y.; Muleri, F.; Pacciani, L.; Rapisarda, M.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy.
[van Baren, C.; Dercksen, J. P. C.; den Herder, J. W.; Frericks, M.; Haas, D.; Hermsen, W.; in't Zand, J. J. M.; Jacobs, H. M.; Jonker, P.; Kuiper, L. M.; Laubert, P. P.; Mehdipour, M.; de la Rie, R.; Zwart, F.] SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Bozzo, E.; Azzarello, P.; Binko, P.; Ferrigno, C.; Guy, L.; Paltani, S.; Rohlfs, R.; Tramacere, A.] Univ Geneva, ISDC, Chemin Ecogia 16, CH-1290 Versoix, Switzerland.
[Alpar, A.; Gogus, E.; Kalemci, E.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[van der Klis, M.; Watts, A.; Cavechi, Y.; Ingram, A.; Markoff, S. B.; Stevens, A. L.; Wijers, R.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Hernanz, M.; Alvarez, L.; Artigues, B.; Caliandro, G. A.; Galvez Sanchez, J. L.; Garcia-Berro, E.; Karelin, D.; Papitto, A.; Portell, J.; Rea, N.; Sala, G.; Tolos, L.] IEEC CSIC UPC UB, Carrer Gran Capita 2, Barcelona 08034, Spain.
[Amati, L.; Fuschino, F.; Grandi, P.; Labanti, C.; Marisaldi, M.; Orlandini, M.; Torresi, E.] INAF IASF Bologna, Via P Gobetti 101, I-40129 Bologna, Italy.
[Amoros, C.; Artigue, R.; Atteia, J. -L.; Barret, D.; Coriat, M.; Cros, A.; Lin, D.; Maestre, S.; Malzac, J.; Mouret, G.; Rambaud, D.; Ramon, P.; Webb, N.] IRAP, Ave Colonel Roche,9 BP 44346, Toulouse, France.
[Andersson, N.; Gandhi, P.] Univ Southampton, Fac Phys & Appl Sci, Southampton SO17 1BJ, Hants, England.
[Antonelli, A.; Cavazzutim, E.; D'Elia, V.; Gendre, B.; Giommi, P.; Pittoril, C.] ASDC, Via Politecn Snc, I-00133 Rome, Italy.
[Balman, S.; Baykal, A.] Middle East Tech Univ, Mah Dumlupinar Blvd 1, TR-06800 Ankara, Turkey.
[Barbera, M.; D'Ai, A.; Di Salvo, T.] Univ Palermo, Dipartimento Fis, Via Archirafi 36, I-90123 Palermo, Italy.
[Belloni, T.; Campana, S.; Tavecchio, F.] INAF OA Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy.
[Ahangarianabhari, M.; Bertuccio, G.; Macera, D.] Politecn Milan, Piazza Leonardo da Vinci 32, I-20133 Milan, Italy.
[Bianchini, A.; Tamburini, F.; Turolla, R.] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Schanne, S.; Bidaud, J. -M. Bonnet; Bouyjou, F.; Chateau, F.; Gevin, O.; Gotz, D.; Gouiffes, C.; Limousin, O.; Le Provost, H.; Rodriguez, J.] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France.
[Santangelo, A.; Boutloukos, S.; Diebold, S.; Doroshenko, V.; Gschwender, M.; Jetter, F.; Klochkov, D.; Kokkotas, K.; Maier, D.; Perinati, E.; Staubert, R.; Suchy, S.; Suleimanovi, V.; Tenzer, C.; Wende, H.] IAAT Univ Tuebingen, Sand 1, D-72076 Tubingen, Germany.
[Braga, J.] INPE, Ave Astronautas 1-758,Jd Granja, BR-12227010 Sao Jose Dos Campos, Brazil.
[Brandt, S.; Budtz-Jorgensen, C.; Chenevez, J.; Hansen, F.; Hornstrup, A.; Kuvvetli, I.; Lund, N.; Mulacova, J.; Neubert, T.; Olsen, P. E. H.] Tech Univ Denmark, Natl Space Inst, Elektrovej Bld 327, DK-2800 Lyngby, Denmark.
[Iwasawa, K.; Migliari, S.; Paredes, J. M.; Ribo, M.] Univ Barcelona IEEC UB, DAM, Marti & Franques 1, E-08028 Barcelona, Spain.
[Iwasawa, K.; Migliari, S.; Paredes, J. M.; Ribo, M.] Univ Barcelona IEEC UB, ICC UB, Marti & Franques 1, E-08028 Barcelona, Spain.
[Bucciantini, N.] INAF, Arcetri Observ, Largo Enrico Fermi 5, I-50125 Florence, Italy.
[Burderi, L.] Cagliari Univ, Str Prov Sestu,KM 1, I-09042 Monserrato, Italy.
[Bursa, M.; Hudec, R.; Karas, V.; Kunneriath, D.; Sochora, V.] Acad Sci Czech Republic, Astron Inst, Fricova 298, CZ-25165 Ondrejov, Czech Republic.
[Fabian, A.] Univ Cambridge, Trinity Lane, Cambridge CB2 1TN, England.
[Pohl, M.; Cadoux, F. R.; Favre, Y.] Univ Geneva, DPNC, Quai Ernest Ansermet 30, CH-1205 Geneva, Switzerland.
[Cais, P.] Lab Astrophys Bordeaux, Rue Observ BP 89, F-33270 Floirac, France.
[Stella, L.; Casella, P.; Israel, G.; Kalamkar, M.; Schneider, R.] INAF OA Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Chakrabarty, D.; Grinberg, V.; Homan, J.; Neilsen, J.; Nowak, M.; Remillard, R.; Weinberg, N.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Zane, S.; Bradley, L.; Coker, J.; Cole, R.; Hailey, M.; Kataria, D.; Kennedy, T.; Lodato, G.; Mignani, R.; Rousseau, A.; Smith, A.; Smith, P. J.; Spencer, A.; Vacchi, A.; Walton, D.; Winter, B.] Univ Coll London, MSSL, Dorking RH5 6NT, Surrey, England.
McGill Univ, 845 Sherbrooke St West, Montreal, PQ H3A 0G4, Canada.
[Cumming, A.; De Martino, D.] INAF OA Capodimonte, I-80131 Naples, Italy.
[Guidorzi, C.] Univ Ferrara, Via Saragat 1, I-44122 Ferrara, Italy.
[Durant, M.] Univ Toronto, Dept Med Biophys, Toronto, ON M4N 3M5, Canada.
[Falanga, M.] ISSI Bern, Hallerstr 6, CH-3012 Bern, Switzerland.
[Feldman, C.; Fraser, G. W.; Martindale, A.; O'Brien, P.; Osborne, J. P.; Pye, J.; Sims, M.; Vaughan, S.] Univ Leicester, Univ Rd, Leicester LE1 5WW, Leics, England.
[Finger, M. H.] Univ Space Res Assoc, 6767 Old Madison Pike,Suite 450, Huntsville, AL 35806 USA.
[Galloway, D. K.; Heger, A.] Monash Univ, Sch Phys, Monash Ctr Astrophys, Clayton, Vic 3800, Australia.
[Galloway, D. K.; Heger, A.] Monash Univ, Sch Math Sci, Clayton, Vic 3800, Australia.
Johns Hopkins Univ, 3400 North Charles St, Baltimore, MD USA.
[Giles, A. B.] Univ Tasmania, Private Bag 37, Hobart, Tas 7001, Australia.
[Gilfanov, M.] MPA Garching, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
Radboud Univ Nijmegen, Heyendaalseweg 135, NL-6500 GL Nijmegen, Netherlands.
[Groot, P.; Hartmann, D. H.] Clemson Univ, Clemson, SC 29634 USA.
[Haswell, C. A.; Norton, A. J.] Open Univ, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Wilson-Hodge, C. A.] NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA.
[Huovelin, J.; Korpela, S.] Univ Helsinki, Div Geophys & Astron, Dept Phys, POB 48, FI-00014 Helsinki, Finland.
Univ Durham, Stockton Rd, Durham DH1 3UP, England.
[Izzo, L.; Penacchioni, A. V.] Sapienza Univ, Ple A Moro 2, I-00185 Rome, Italy.
[Izzo, L.; Penacchioni, A. V.] ICRA, Ple A Moro 2, I-00185 Rome, Italy.
Univ Iowa, Van Allen Hall, Iowa City, IA 52242 USA.
[Brown, E.; Kaaret, P.; Miller, J. M.; Schatz, H.] Michigan State Univ, 567 Wilson Rd, E Lansing, MI 48824 USA.
[Czerny, B.; Haensel, P.; Kluzniak, W.; Manousakis, A.; Rozanska, A.; Rudak, B.; Sobolewska, M.; Uter, P.; Vincent, F. H.; Zdunik, L.; Zdziarski, A.] Copernicus Astron Ctr, Bartycka 18, Warsaw, Poland.
[Kouveliotou, C.] George Washington Univ, 2121 I St NW, Washington, DC 20052 USA.
[Lai, D.] Cornell Univ, Space Bldg, Ithaca, NY 14853 USA.
[Lamb, F. K.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Lodato, G.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.
[Longo, F.] Univ Trieste, Via Alfonso Valerio 32, I-34128 Trieste, Italy.
[Grassi, M.; Malcovati, P.] Univ Pavia, Corso Str Nuova 65, I-27100 Pavia, Italy.
[Cusumano, G.; De Pasquale, M.; Mineo, T.; Romano, P.; Vercellone, S.] INAF IASF, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[Smith, D. M.; Woosley, S. E.] Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA.
[Bianchi, S.; La Franca, F.; Marinucci, A.] Univ Roma III, Via Vasca Navale 84, I-00146 Rome, Italy.
[Melatos, A.] Univ Melbourne, Swanston St, Parkville, Vic 3052, Australia.
[Mendez, M.; Sanna, A.; Soleri, P.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Gezari, S.; Miller, M. C.; Reynolds, C.; Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reina Aranda, M.; Sabau-Graziati, L.] Natl Inst Aerosp Technol INTA, Carretera Ajalvir Km 4, Torrejon De Ardoz 28850, Spain.
[Morsink, S.] Univ Alberta, 85 Ave 116 St NW, Edmonton, AB T6G 2R3, Canada.
[Motch, C.] Observ Astron, 11 Rue Univ, F-67000 Strasbourg, France.
[Mouchet, M.] Univ Paris Diderot, 5 Rue Thomas Mann, F-75205 Paris 13, France.
INAF OA Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy.
[Orleanski, P.; Michalska, M.; Wawrzaszek, R.] Space Res Ctr, Bartycka 18A, Warsaw, Poland.
[Osten, R.] Space Telescope Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Ozel, F.; Psaltis, D.] Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Paul, B.] Raman Res Inst, CV Raman Ave, Sadashivanagar 560080, India.
[Hudec, R.; Petracek, V.] Czech Tech Univ, Zikova 1903-4, CZ-16636 Prague 6, Czech Republic.
[Poutanen, J.] Univ Turku, Tuorla Observ, Vaisalantie 20, FIN-21500 Piikkio, Finland.
[Ramsay, G.] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
[Mihara, T.; Rachevski, A.; Zampa, G.; Zampa, N.] Ist Nazl Fis Nucl, Via A Valerio 2, I-34127 Trieste, Italy.
[Ray, P. S.; Wood, K.] NRL, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Reddy, S.] Univ Washington, Inst Nucl Theory, Seattle, WA 98195 USA.
[Papadakis, I.; Reig, P.] Univ Crete, Phys Dept, GR-71003 Iraklion, Greece.
[Casares, J.; Cornelisse, R.; Linares, M.; Rodriguez-Gil, P.] Inst Astrofis Canarias, Via Lactea S-N, E-38205 Tenerife, Spain.
[Patruno, A.; Rossi, E. M. R.] Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Ryde, F.] KTH Royal Inst Technol, Valhallavagen 79, S-10044 Stockholm, Sweden.
[De Luca, A.; Esposito, P.; Marelli, J. MargueronM.; Mereghetti, S.; Salvaterra, R.; Salvetti, D.] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy.
[Bakala, P.; Doyle, G.; Goluchova, K.; Schee, J.; Stuchlik, Z.; Torok, G.] Silesian Univ Opava, Rybnicku 626-1, Opava 74601, Czech Republic.
[Wilms, J.; Kreykenbohm, I.; Schmid, C.; Wille, M.] Univ Erlangen Nurnberg, Schlosspl 4, D-91054 Erlangen, Germany.
[Hebeler, K.; Schwenk, A.] GSI Helmholtzzentrum Schwerionenforsch GmbH, ExtreMe Matter Inst EMMI, D-64291 Darmstadt, Germany.
[Schwope, A. D.; Traulsen, I.] Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany.
[Shearer, A.] Natl Univ Ireland Galway, Univ Rd, Galway, Ireland.
[Stappers, B.] Univ Manchester, Booth St West, Manchester M15 6PB, Lancs, England.
[Stergioulas, N.] Aristotle Univ Thessaloniki, Thessaloniki, Greece.
[Drake, S. A.; Enoto, T.; Kowalski, A. F.; Mahmoodifar, S.; Schnittman, J. D.; Strohmayer, T. E.] Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Takahashi, T.; Watanabe, S.] ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Negueruela, I.; Pons, J.; Torrejon, J. M.] Univ Alicante, Carretera San Vicente del Raspeig, St Vicent Del Raspeig 03690, Spain.
[Torres, D. F.] ICREA, Passeig Lluis Co 23, Barcelona 08010, Spain.
[Uttley, P.; Vrba, V.] Acad Sci Czech Republic, Phys Inst, Slovance 1999-2, CZ-18221 Prague 8, Czech Republic.
[Wheatley, P.] Univ Warwick, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Bocchino, F.; Orio, M.; Zampieri, L.] INAF OA Padova, Vicolo Osservatorio 5, Padua, Italy.
[Zhang, B.] Univ Nevada, Las Vegas, NV 89012 USA.
[Turriziani, S.] Univ Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy.
[D'Ammando, F.; Giovannini, G.; Giroletti, M.; Orienti, M.; Prandoni, I.] INAF IRA Bologna, Via P Gobetti 101, I-40129 Bologna, Italy.
[Baldazzi, G.; D'Ammando, F.] Univ Bologna, Dept Phys, Vle Berti Pichat 6-2, I-40127 Bologna, Italy.
[Baldazzi, G.; D'Ammando, F.] Ist Nazl Fis Nucl, Sect Bologna, Vle Berti Pichat 6-2, I-40127 Bologna, Italy.
[Rodriguez-Gil, P.] Univ La Laguna, Dept Astrophys, E-38206 San Cristobal la Laguna, Santa Cruz De T, Spain.
[Goldwurm, A.; Lachaud, C.; Lebrun, F.] Univ Paris Diderot, CEA Irfu, Observ Paris, APC,UMR 7164,CNRS N2P3,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
[Barbera, M.; Collura, A.] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Altamirano, D.; Emmanoulopoulos, D.; McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Linares, M.; Mignani, R.] Univ Zielona Gora, Kepler Inst Astron, Lubuska 2, PL-65265 Zielona Gora, Poland.
[Markowitz, A.] Univ Calif San Diego, Mail Code 0424, La Jolla, CA 92093 USA.
[Cackett, E.] Univ Wisconsin, Dept Astron, 475 N Charter Str, Madison, WI 53706 USA.
[Cackett, E.] Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA.
[Miniuttill, G.] Ctr Astrobiol CSIC INTA, POB 78, E-28691 Madrid, Spain.
[Reig, P.] Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece.
[Bodin, P.; Seyler, J. -Y.] CNES, 18 Ave Edouard Belin, F-31400 Toulouse, France.
[Burgay, M.; Pellizzoni, A.; Possenti, A.; Riggio, A.] INAF OA Cagliari, Str 54, I-09012 Capoterra, Italy.
[Agudo, I.; Castro-Tirado, A. J.; Perez-Torres, M.] Inst Astrofis Andalucia, Glorieta Astron IAAC CSIC S-N, E-18008 Granada, Spain.
[Bombaci, I.; Shore, S.] Univ Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
[Johannsen, T.] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada.
[Paolillo, M.] Univ Napoli Fedelico II, Dipartimento Sci Fis, CU Monte St Angelo,Via Cintia Ed 6, I-80126 Naples, Italy.
[Mandel, I.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Prakash, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Greiner, J.; Kanbach, G.; Scaringi, S.] Max Planck Inst Extraterr Phys, Postfach 1603, D-85740 Garching, Germany.
[Rezzolla, L.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Muhlenberg 1, D-14476 Golm, Germany.
[Blay, P.; Cerda-Duran, P.; Gabler, M.] Univ Valencia, Ave Vicente Blasco Ibanez 13, Valencia 46010, Spain.
[Jose, J.] Tech Univ Catalonia, C Jordi Girona 31, Barcelona 08034, Spain.
[Johannsen, T.] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada.
[Behar, O.; Evangelista, V.; Gualtieri, L.] Sapienza Univ, Ple A Moro 2, I-00185 Rome, Italy.
[Tauris, T.] Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
[Maccarone, T. J.] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA.
[Bhattacharyya, S.] Tata Inst Fundamental Res, 1 Homi Bhabha Rd, Mumbai 400005, Maharashtra, India.
[Finger, M.] Charles Univ Prague, Fac Math & Phys, V Holesovickach 2, CZ-18000 Prague, Czech Republic.
[Sandberg, J.] Jorgen Sandberg Consulting, Copenhagen, Denmark.
[Erkut, M. H.] Istanbul Kultur Univ, Atakoy Campus, TR-34156 Istanbul, Turkey.
[Perez, M. A.] Univ Salamanca, Fac Ciencias Trilingue, Fundamental Phys Dept, Plaza Merced S-N, E-37008 Salamanca, Spain.
[Albertus, C.] Univ Granada, Fac Ciencias, Dept Fis Atom Mol & Nucl, E-18071 Granada, Spain.
[Rios, A.] Univ Surrey, Guildford GU2 7XH, Surrey, England.
[Alford, M.] Washington Univ, Dept Phys, Compton Hall,One Brookings Dr,Campus Box 1105, St Louis, MO 63130 USA.
[Fender, R.; Motta, S.; Munoz-Darias, T.] Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
[Patruno, A.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Mangano, V.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Zhang, S. -N.; Cao, X.; Chen, Y.; Dong, Y.; Lu, F.; Qu, J.; Song, L.; Varniere, P.; Wang, J.; Zhang, S.] Inst High Energy Phys, 19B YuquanLu, Beijing 1000049, Peoples R China.
[Yu, W.; Yuan, F.] Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China.
[Peng, H.] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China.
[Peng, H.] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China.
[Wang, Z.] Tongji Univ, Inst Precis Opt Engn, Dept Phys, Shanghai 200092, Peoples R China.
[Gou, L.; Yuan, W.; Zhang, C.] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing, Peoples R China.
[Chen, Y.; Dai, Z.; Li, X.] Nanjing Univ, 22 Hankou Rd, Nanjing 210093, Jiangsu, Peoples R China.
[Cui, W.] Purdue Univ, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
[Chen, C.] Shanghai Acad Spaceflight Technol, Yangpu City Ind Pk,135,Guowei Rd, Shanghai, Peoples R China.
[Gao, Z.] China Acad Space Technol, Beijing, Peoples R China.
[Yuan, Y.] Univ Sci & Technol China, 96 JinZhai Rd, Hefei 230026, Anhui, Peoples R China.
[Xu, R.] Peking Univ, 5 Yiheyuan Rd, Beijing 100871, Peoples R China.
[Liang, E.] Guangxi Univ, 188 East Daxue Rd, Nanning 530006, Guangxi, Peoples R China.
[Wu, X.] Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China.
[Hempel, M.; Thielemann, F. K.] Univ Basel, Dept Phys, Klingelbergstr 82, CH-4056 Basel, Switzerland.
[Zech, A.] Univ Paris Diderot, LUTH, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Margueron, J.; Oertel, M.] IPN Lyon, 4 Rue Enrico Fermi, F-69622 Lyon, France.
[Kurkela, A.] CERN, CH-1211 Geneva 23, Switzerland.
[Vietri, M.] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
[Bernardini, F.; Russell, D. M.] NYUAD, POB 129188, Abu Dhabi, U Arab Emirates.
[Ballantyne, D. R.; Keek, L.] Georgia Inst Technol, North Ave NW, Atlanta, GA 30332 USA.
[Paragi, Z.] JIVE, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Komossa, S.; Savolainen, T.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Endenich, Germany.
[Komossa, S.; Savolainen, T.] Max Planck Inst Radioastron, Postfach 20 24, D-53010 Bonn, Germany.
[Nucita, A.] Univ Salento, Dept Math & Phys, Via Arnesano,CP 193, I-73100 Lecce, Italy.
[Nucita, A.] Ist Nazl Fis Nucl, Via Arnesano,CP 193, I-73100 Lecce, Italy.
[Koerding, E.] Radboud Univ Nijmegen, Comeniuslaan 4, NL-6525 HP Nijmegen, Netherlands.
[Bode, M.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
[Begelman, M.] Univ Colorado, JILA, 440 UCB, Boulder, CO 80309 USA.
[Tiengo, A.] IUSS Ist Univ Studi Super Pavia, Palazzo Broletto Piazza Vittoria 15, I-27100 Pavia, Italy.
[Slowikowska, A.] Univ Zielona Gora, PL-65417 Zielona Gora, Poland.
[Costamante, L.] Univ Perugia, Dept Phys, I-06123 Perugia, Italy.
[Stamerra, A.] INAF IFSI Torino, Corso Fiume 4, I-10133 Turin, Italy.
[Malone, C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Paerels, F.] Columbia Univ, 116th St & Broadway, New York, NY 10027 USA.
[Serino, M.] RIKEN, Wako, Saitama, Japan.
[Zingale, M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Postnov, K.; Shakura, N.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Inam, S. C.] Baskent Univ, Dept Elect & Elect Engn, Ankara, Turkey.
[Behar, E.; Peretz, U.] Technion Israel Inst Technol, IL-3200003 Haifa, Israel.
[Behar, E.; Peretz, U.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Hamuguchi, K.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA.
[Hamuguchi, K.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Guedel, M.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Stratta, G.] Univ Urbino Carlo Bo, Piazza Repubbl 13, I-61029 Urbino, Italy.
[Jenke, P. A.] Univ Alabama, 301 Sparkman Dr, Huntsville, AL 35899 USA.
[Pederiva, F.] Univ Trento, Dipartimento Fis, Via Sommar, I-38123 Trento, Italy.
[Baldo, M.] Ist Nazl Fis Nucl, Via Santa Sofia 64, I-95123 Catania, Italy.
[Rischke, D. H.; Schaffner-Bielich, J.; Sedrakian, A.] Goethe Univ, Inst Theoret Phys, D-60438 Frankfurt, Germany.
[Type, S.] GSI Helmholtzzentrum Schwerionenforsch GmbH, Planckstr 1, D-64291 Darmstadt, Germany.
[Buballa, M.; Hebeler, K.; Martinez, G.; Schwenk, A.] Tech Univ Darmstadt, Inst Kernphys, D-64289 Darmstadt, Germany.
[Chamel, N.] Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium.
[Sakamoto, T.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2525258, Japan.
[Briggs, M. S.] Univ Alabama, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Tamura, H.] Tohoku Univ, Dept Phys, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Degenaar, N.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Chernyakova, M.] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland.
[Celestin, S.] Univ Orleans, CNRS, Lab Phys & Chem Environm & Space LPC2E, F-45067 Orleans, France.
[Fullekrug, M.] Univ Bath, Dept Elect & Elect Engn, Ctr Space Atmospher & Ocean Sci, Bath, Avon, England.
[Liu, L. -P.; Xiao, L.] China Acad Space Technol China, Beijing, Peoples R China.
[Medina-Tanco, G.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Apartado Postal 70-543,Ciudad Univ, Mexico City, DF 04510, Mexico.
[Peterson, B. M.] Ohio State Univ, McPherson Lab 4055, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Huppenkothen, D.] NYU, Ctr Data Sci, 726 Broadway, New York, NY 10003 USA.
[Steiner, A. W.] Univ Tennessee, Knoxville, TN 37996 USA.
[Bellutti, P.; Borghi, G.; Ficorella, F.; Picciotto, A.; Piemonte, C.; Zorzi, N.] Fdn Bruno Kessler, Via Sommar 18, I-38123 Trento, Italy.
Trento Inst Fundamental Phys & Applicat, Via Sommar 14, I-38123 Trento, Italy.
RP Feroci, M (reprint author), IAPS INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM marco.feroci@inaf.it
RI Malcovati, Piero/S-2458-2016; Bursa, Michal/G-9004-2014;
OI Ray, Paul/0000-0002-5297-5278; TORRESI, ELEONORA/0000-0002-5201-010X;
Paolillo, Maurizio/0000-0003-4210-7693; Malcovati,
Piero/0000-0001-6514-9672; Sanna, Andrea/0000-0002-0118-2649; de
Martino, Domitilla/0000-0002-5069-4202; Groot, Paul/0000-0002-4488-726X;
Gendre, Bruce/0000-0002-9077-2025; orienti, monica/0000-0003-4470-7094;
Stevens, Abigail/0000-0002-5041-3079; Esposito,
Paolo/0000-0003-4849-5092; Poutanen, Juri/0000-0002-0983-0049;
Tramacere, Andrea/0000-0002-8186-3793; Wheatley,
Peter/0000-0003-1452-2240
NR 27
TC 0
Z9 0
U1 13
U2 13
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99051R-1
DI 10.1117/12.2233161
PN 1
PG 20
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500048
ER
PT S
AU Grant, CE
Bautz, MW
Durham, RN
Plucinsky, PP
AF Grant, Catherine E.
Bautz, Marshall W.
Durham, R. Nick
Plucinsky, Paul P.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Evolution of temperature-dependent charge transfer inefficiency
correction for ACIS on the Chandra X-ray Observatory
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Chandra X-ray Observatory; ACIS; radiation damage; charge transfer
inefficiency; CCDs; X-rays
ID CCD IMAGING SPECTROMETER
AB As the Advanced CCD Imaging Spectrometer (ACIS) on the Chandra X-ray Observatory enters its seventeenth year of operation, it continues to perform well and produce spectacular scientific results. The response of ACIS has evolved over the lifetime of the observatory due to radiation damage and aging of the spacecraft. The ACIS instrument team developed a software tool which applies a correction to each X-ray event and mitigates charge transfer inefficiency (CTI) and spectral resolution degradation. The behavior of the charge traps that cause CTI are temperature dependent, however, and warmer temperatures reduce the effectiveness of the correction algorithm. As the insulation on the exterior of the spacecraft degrades with time, the temperature of the ACIS focal plane can increase by several degrees for some spacecraft orientations. A temperature-dependent component was added to the CTI correction algorithm in 2010. We present an evaluation of the effectiveness of this algorithm as the radiation damage and thermal environment continue to evolve and suggest updates to improve the calibration fidelity.
C1 [Grant, Catherine E.; Bautz, Marshall W.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Durham, R. Nick; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Grant, CE (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM cgrant@mit.edu
NR 8
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990545-1
DI 10.1117/12.2233424
PN 1
PG 11
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500123
ER
PT S
AU Mccoy, J
McEntaffer, R
Deroo, C
AF McCoy, Jake
McEntaffer, Randall
DeRoo, Casey
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI New lithographic techniques for X-ray spectroscopy
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray optics; diffraction gratings; off-plane gratings; spectroscopy;
nanofabrication; electron-beam lithography; thermally activated
selective topography equilibration; substrate conformal imprint
lithography
ID NANOIMPRINT LITHOGRAPHY; GRATINGS; FABRICATION; REPLICATION; RESIST
AB Off-plane reflection gratings require high-fidelity, custom groove profiles to perform with high spectral resolution in a Wolter-I optical system. This places a premium on exploring lithographic techniques in nanofabrication to produce state-of-the-art gratings. The fabrication recipe currently being pursued involves electron-beam lithography (EBL) and reactive ion etching (RIE) to define the groove profile, wet anisotropic etching in silicon to achieve blazed grooves and UV-nanoimprint lithography (UV-NIL) to replicate the final product. A process involving grayscale EBL and thermal reflow known as thermally activated selective topography equilibration (TASTE) is also being investigated as an alternative method to fabricate these gratings. However, a master grating fabricated entirely in soft polymeric resist through the TASTE process requires imprinting procedures other than UV-NIL to explored. A commerically available process called substrate conformal imprint lithography (SCIL) has been identified as a possible solution to this problem. SCIL also has the ability to replicate etched silicon gratings with reduced trapped air defects as compared to UV-NIL, where it is difficult to achieve conformal contact over large areas. As a result, SCIL has the potential to replace UV-NIL in the current grating fabrication recipe.
C1 [McCoy, Jake; McEntaffer, Randall] Penn State Univ, University Pk, PA 16802 USA.
[DeRoo, Casey] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Mccoy, J (reprint author), Penn State Univ, University Pk, PA 16802 USA.
EM jam1117@psu.edu
NR 34
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990524
DI 10.1117/12.2232072
PN 1
PG 10
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500058
ER
PT S
AU Plucinsky, PP
Bogdan, A
Germain, G
Marshall, HL
AF Plucinsky, Paul P.
Bogdan, Akos
Germain, Gregg
Marshall, Herman L.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI The Evolution of the ACIS Contamination Layer over the 16 Year Mission
of the Chandra X-ray Observatory
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-rays; CCDs; Chandra X-ray Observatory; ACIS; contamination
ID CCD IMAGING SPECTROMETER; RADIATION-DAMAGE; CALIBRATION; INSTRUMENT
AB The Chandra X-ray Observatory (CXO) was launched 16 years ago and has been delivering spectacular science over the course of its mission. The Advanced CCD Imager Spectrometer (ACIS) is the prime instrument on the satellite, conducting over 90% of the observations. The CCDs operate at a temperature of -120 C and the optical blocking filter (OBF) in front of the CCDs is at a temperature of approximately -60 C. The surface of the OBF has accumulated a layer of contamination over the course of the mission, as it is the coldest surface exposed to the interior to the spacecraft. We have been characterizing the thickness, chemical composition, and spatial distribution of the contamination layer as a function of time over the mission. All three have exhibited significant changes with time. The calibration team within the Chandra X-ray Center (CXC) generates calibration files that describe the additional absorption produced by the contamination layer as a function of time, position, and energy. We have verified the accuracy of this contamination file for the on-axis aimpoints using the standard model spectrum for the Supernova Remnant 1E 0102.2-7219 in the Small Magellanic Cloud developed by the International Consortium for High Energy Calibration (IACHEC), but we show the model is less accurate for the off-axis positions after 2013. In 2015, the ACIS Detector Housing heater was turned on to increase the temperature of the OBF in the hope that the accumulation rate of the contamination layer would decrease. We show that the accumulation rate of the contaminant is unchanged since the DH heater was turned on.
C1 [Plucinsky, Paul P.; Bogdan, Akos; Germain, Gregg] Harvard Smithsonian Ctr Astrophys, MS-3,60 Garden St, Cambridge, MA 02138 USA.
[Marshall, Herman L.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Plucinsky, PP (reprint author), Harvard Smithsonian Ctr Astrophys, MS-3,60 Garden St, Cambridge, MA 02138 USA.
EM pplucinsky@cfa.harvard.edu
NR 20
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990544
DI 10.1117/12.2233837
PN 1
PG 15
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500122
ER
PT S
AU Smith, RK
Abraham, MH
Allured, R
Bautz, M
Bookbinder, J
Bregman, JN
Brenneman, L
Brickhouse, NS
Burrows, DN
Burwitz, V
Carvalho, R
Cheimets, PN
Costantini, E
Dawson, S
Deroo, C
Falcone, A
Foster, AR
Grant, CE
Heilmann, RK
Hertz, E
Hine, B
Huenemoerder, D
Kaastra, JS
Madsen, KK
McEntaffer, RL
Miller, ED
Miller, J
Morse, E
Mushotzky, R
Nandra, K
Nowak, M
Paerels, E
Petre, R
Plice, L
Poppenhaeger, K
Ptak, A
Reid, P
Sanders, J
Schattenburg, ML
Schulz, N
Smale, A
Temi, P
Valencic, L
Walker, S
Willingale, R
Wilms, J
Wolk, SJ
AF Smith, R. K.
Abraham, M. H.
Allured, R.
Bautz, M.
Bookbinder, J.
Bregman, J. N.
Brenneman, L.
Brickhouse, N. S.
Burrows, D. N.
Burwitz, V.
Carvalho, R.
Cheimets, P. N.
Costantini, E.
Dawson, S.
DeRoo, C.
Falcone, A.
Foster, A. R.
Grant, C. E.
Heilmann, R. K.
Hertz, E.
Hine, B.
Huenemoerder, D.
Kaastra, J. S.
Madsen, K. K.
McEntaffer, R. L.
Miller, E. D.
Miller, J.
Morse, E.
Mushotzky, R.
Nandra, K.
Nowak, M.
Paerels, E.
Petre, R.
Plice, L.
Poppenhaeger, K.
Ptak, A.
Reid, P.
Sanders, J.
Schattenburg, M. L.
Schulz, N.
Smale, A.
Temi, P.
Valencic, L.
Walker, S.
Willingale, R.
Wilms, J.
Wolk, S. J.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI Arcus: The X-ray Grating Spectrometer Explorer
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Gratings; X-rays: spectroscopy; Instrumentation
ID SPECTROSCOPY; ABSORPTION
AB Arcus will be proposed to the NASA Explorer program as a free-flying satellite mission that will enable high-resolution soft X-ray spectroscopy (8-50 angstrom) with unprecedented sensitivity effective areas of >500 sq cm and spectral resolution >2500. The Arcus key science goals are (1) to determine how baryons cycle in and out of galaxies by measuring the effects of structure formation imprinted upon the hot gas that is predicted to lie in extended halos around galaxies, groups, and clusters, (2) to determine how black holes influence their surroundings by tracing the propagation of out flowing mass, energy and momentum from the vicinity of the black hole out to large scales and (3) to understand how accretion forms and evolves stars and circumstellar disks by observing hot infalling and outflowing gas in these systems. Arcus relies upon grazing-incidence silicon pore X-ray optics with the same 12m focal length (achieved using an extendable optical bench) that will be used for the ESA Athena mission. The focused X-rays from these optics will then be diffracted by high-efficiency off-plane reflection gratings that have already been demonstrated on sub-orbital rocket flights, imaging the results with flight-proven CCD detectors and electronics. The power and telemetry requirements on the spacecraft are modest. The majority of mission operations will not be complex, as most observations will be long (similar to 100 ksec), uninterrupted, and pre-planned, although there will be limited capabilities to observe targets of opportunity, such as tidal disruption events or supernovae with a 3-5 day turnaround. After the end of prime science, we plan to allow guest observations to maximize the science return of Arcus to the community.
C1 [Smith, R. K.; Allured, R.; Brenneman, L.; Brickhouse, N. S.; Cheimets, P. N.; DeRoo, C.; Foster, A. R.; Hertz, E.; Reid, P.; Wolk, S. J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Abraham, M. H.] Aerosp Corp, El Segundo, CA 90245 USA.
[Bautz, M.; Grant, C. E.; Heilmann, R. K.; Huenemoerder, D.; Miller, E. D.; Miller, J.; Nowak, M.; Schattenburg, M. L.; Schulz, N.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Bookbinder, J.; Carvalho, R.; Dawson, S.; Hine, B.; Plice, L.; Temi, P.; Walker, S.] NASA, Ames Res Ctr, Moffett Field, CA USA.
[Bregman, J. N.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Burrows, D. N.; Falcone, A.; McEntaffer, R. L.] Penn State Univ, State Coll, PA USA.
[Burwitz, V.; Nandra, K.; Sanders, J.] Max Planck Inst Extraterr Phys, Garching, Germany.
[Costantini, E.; Kaastra, J. S.] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Madsen, K. K.] CALTECH, Pasadena, CA 91125 USA.
[Morse, E.] Orbital ATK, Dulles, VA USA.
[Mushotzky, R.] Univ Maryland, College Pk, MD 20742 USA.
[Paerels, E.] Columbia Univ, New York, NY USA.
[Petre, R.; Ptak, A.; Smale, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Poppenhaeger, K.] Queens Univ Belfast, Belfast, Antrim, North Ireland.
[Valencic, L.] Johns Hopkins Univ, Baltimore, MD USA.
[Willingale, R.] Univ Leicester, Leicester, Leics, England.
[Wilms, J.] Friedrich Alexander Univ, Erlangen, Germany.
RP Smith, RK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM rsmith@cfa.harvard.edu
RI Heilmann, Ralf/D-4680-2009
NR 13
TC 0
Z9 0
U1 2
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99054M
DI 10.1117/12.2231778
PN 1
PG 7
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500133
ER
PT S
AU Soffitta, P
Bellazzini, R
Bozzo, E
Burwitz, V
Castro-Tirado, AJ
Costa, E
Courvoisier, T
Feng, H
Gburek, S
Goosmann, R
Karas, V
Matt, G
Muleri, F
Nandra, K
Pearce, M
Poutanen, J
Reglero, V
Maria, DS
Santangelo, A
Tagliaferri, G
Tenzer, C
Vink, J
Weisskopf, MC
Zane, S
Agudo, I
Antonelli, A
Attina, P
Baldini, L
Bykov, A
Carpentiero, R
Cavazzuti, E
Churazov, E
Del Monte, E
De Martino, D
Donnarunnna, I
Doroslienko, V
Evangelista, Y
Ferreira, I
Gallo, E
Grosso, N
Kaaret, P
Kuulkers, E
Laranaga, J
Latronico, L
Lumb, DH
Macian, J
Malzac, J
Marin, F
Massaro, E
Minuti, M
Mundell, C
Ness, JU
Oosterbroek, T
Paltani, S
Pareschi, G
Perna, R
Petrucci, PO
Pinazo, HB
Pinchera, M
Rodriguez, JP
Roncadelli, M
Santovincenzo, A
Sazonov, S
Sgro, C
Spiga, D
Svoboda, J
Theobald, C
Theodorou, T
Turolla, R
de Ona, EW
Winter, B
Akbar, AM
Allan, H
Aloisio, B
Altamirano, D
Amati, L
Amato, E
Angelakis, E
Arezu, J
Atteia, JL
Axelsson, M
Bachetti, M
Ballo, L
Balman, S
Bandiera, R
Barcons, N
Basso, S
Baykal, A
Backer, W
Behar, E
Beheshtipour, B
Belmont, R
Berger, L
Bernardini, F
Bianchi, S
Bisnovatvi-Kogan, G
Blasi, P
Blay, P
Bodaghee, A
Boer, M
Boettcher, M
Bogdanov, S
Bombaci, I
Bonino, R
Braga, J
Brandt, W
Brez, A
Bucciantini, N
Burderi, L
Caiazzo, I
Campana, R
Campana, S
Capitanio, F
Cappi, M
Cardillo, M
Casella, P
Catmabacak, O
Cenko, B
Cerda-Duran, P
Cerruti, C
Chaty, S
Chauvin, M
Chen, V
Chenevez, J
Chernyakova, M
Teddy, CCC
Christodoulou, D
Connell, P
Corbet, R
Zelati, FC
Covino, S
Cui, W
Cusumano, G
D'Ai, A
D'Ammando, F
Dadina, M
De Rosa, A
De Ruvo, L
Degenaar, N
Del Santo, M
Del Zanna, L
Dewangan, G
Di Cosimo, S
Di Lalla, N
Di Persio, G
Di Salvo, T
Dias, T
Done, C
Dovciak, M
Doyle, G
Ducci, L
Elsner, R
Enoto, T
Escada, J
Esposito, P
Eyles, C
Fabiani, S
Falanga, M
Falocco, S
Fan, Y
Fender, R
Feroci, M
Ferrigno, C
Forman, W
Foschini, L
Fragile, C
Fuerst, F
Fujita, Y
Gasent-Blesa, JL
Gelfand, J
Gendre, B
Ghirlanda, G
Ghisellini, G
Giroletti, M
Goetz, D
Gomez, JL
Gonzalez, D
Gonzalcz-Riestra, R
Gotthelf, E
Gou, L
Grandi, P
Grinberg, V
Grise, F
Guidorzi, C
Gurlebeck, N
Guver, T
Haggard, D
Hardcastle, M
Hartmann, D
Haswell, C
Heger, A
Hernanz, M
Heyl, J
Ho, L
Hoormann, J
Horak, J
Huovelin, J
Huppenkothen, D
Iaria, R
Inam, SC
Ingram, A
Israel, G
Izzo, L
Burgess, M
Jackson, M
Ji, L
Ji, L
Jiang, J
Johannsen, T
Jones, C
Jorstad, S
Kajava, JJE
Kalamkar, M
Kalemci, L
Kallman, T
Kamble, A
Kislat, F
Kiss, M
Klochkov, D
Koerding, E
Kolehmainen, M
Koljonen, K
Komossa, S
Kong, A
Korpela, S
Kowalinski, M
Krawczynski, H
Kreykenbohm, I
Kuss, M
Lai, D
Lan, M
Larsson, J
Laycock, S
Lazzati, D
Leahy, D
Li, H
Li, J
Li, LX
Li, T
Li, Z
Linares, M
Lister, M
Liu, H
Lodato, G
Lohfink, A
Longo, F
Luna, G
Lutovinov, A
Mahmoodifar, S
Maia, J
Mainieri, V
Maitra, C
Maitra, D
Majczyna, A
Maldera, S
Malyshev, D
Manfreda, A
Manousakis, A
Manuel, R
Margutti, R
Marinucci, A
Markoff, S
Marschcr, A
Marshall, H
Massaro, F
McLaughlin, M
Medina-Tanco, G
Mehdipour, N
Middleton, N
Mignari, R
Mimica, P
Mineo, T
Mingo, B
Miniutti, G
Mirac, SM
Morlino, G
Motlagli, AV
Motta, SE
Muslitukov, A
Nagataki, S
Nardini, F
Nattila, J
Navarro, GJ
Negri, B
Negro, M
Nenonen, S
Neustroev, V
Nicastro, F
Norton, A
Nucita, A
O'Brien, P
O'Dell, S
Odaka, H
Olmi, B
Omodei, N
Orienti, M
Orlandini, M
Osborne, J
Pacciani, L
Paliya, VS
Papadakis, I
Papitto, A
Paragi, Z
Pascal, P
Paul, B
Pavan, L
Pellizzoni, A
Perinati, E
Pesce-Rollins, M
Piconcelli, E
Pili, AG
Pilia, M
Pohl, M
Ponti, G
Porquet, D
Possenti, A
Postnov, K
Prandoni, I
Produit, N
Puehlhofer, G
Ramsey, B
Razzano, M
Rea, N
Reig, P
Reinsch, K
Reiprich, T
Reynolds, M
Risaliti, G
Roberts, T
Rodriguez, J
Rossi, ME
Rosswog, S
Rozanska, A
Rubini, A
Rudak, B
Russell, D
Ryde, F
Sabatini, S
Sala, G
Salvati, M
Sasaki, M
Savolainen, T
Saxton, R
Scaringi, S
Schawinski, K
Schulz, NS
Schwope, A
Severgnini, P
Sharon, M
Shaw, A
Shearer, A
Shesheng, X
Shih, IC
Silva, K
Silva, R
Silver, E
Sniale, A
Spada, F
Spandre, G
Stamerra, A
Stappers, B
Starrfield, S
Stawarz, L
Stergioulas, N
Stevens, A
Stiele, H
Suleimanov, V
Sunyaev, R
Slowikowska, A
Tamborra, F
Tavecchio, F
Taverna, R
Tiengo, A
Tolos, L
Tombesi, F
Tomsick, J
Tong, H
Torok, G
Torres, DF
Tortosa, A
Tramacere, A
Trimble, V
Trinchieri, G
Tsygankov, S
Tuerler, M
Turriziani, S
Ursini, F
Uttley, P
Varniere, P
Vincent, F
Vurgun, E
Wang, C
Wang, Z
Watts, A
Wheeler, JC
Wiersema, K
Wijnands, R
Wilms, J
Wolter, A
Wood, K
Wu, K
Wu, X
Xiangyu, W
Xie, F
Xu, R
Yan, SP
Yang, J
Vu, W
Yuan, F
Zajczyk, A
Zanetti, D
Zanin, R
Zanni, C
Zappacosta, L
Zdziarski, AA
Zech, A
Zhang, H
Zhang, S
Zhang, S
Zhang, W
Zoghbi, A
AF Soffitta, P.
Bellazzini, R.
Bozzo, E.
Burwitz, V
Castro-Tirado, A. J.
Costa, E.
Courvoisier, T.
Feng, H.
Gburek, S.
Goosmann, R.
Karas, V
Matt, G.
Muleri, F.
Nandra, K.
Pearce, M.
Poutanen, J.
Reglero, V
Maria, Sabau D.
Santangelo, A.
Tagliaferri, G.
Tenzer, C.
Vink, J.
Weisskopf, M. C.
Zane, S.
Agudo, I
Antonelli, A.
Attina, P.
Baldini, L.
Bykov, A.
Carpentiero, R.
Cavazzuti, E.
Churazov, E.
Del Monte, E.
De Martino, D.
Donnarunnna, I
Doroslienko, V
Evangelista, Y.
Ferreira, I
Gallo, E.
Grosso, N.
Kaaret, P.
Kuulkers, E.
Laranaga, J.
Latronico, L.
Lumb, D. H.
Macian, J.
Malzac, J.
Marin, F.
Massaro, E.
Minuti, M.
Mundell, C.
Ness, J. U.
Oosterbroek, T.
Paltani, S.
Pareschi, G.
Perna, R.
Petrucci, P. -O
Pinazo, H. B.
Pinchera, M.
Rodriguez, J. P.
Roncadelli, M.
Santovincenzo, A.
Sazonov, S.
Sgro, C.
Spiga, D.
Svoboda, J.
Theobald, C.
Theodorou, T.
Turolla, R.
de Ona, Wilhelmi E.
Winter, B.
Akbar, A. M.
Allan, H.
Aloisio, B.
Altamirano, D.
Amati, L.
Amato, E.
Angelakis, E.
Arezu, J.
Atteia, J. -L
Axelsson, M.
Bachetti, M.
Ballo, L.
Balman, S.
Bandiera, R.
Barcons, N.
Basso, S.
Baykal, Altan
Backer, W.
Behar, E.
Beheshtipour, B.
Belmont, R.
Berger, L.
Bernardini, F.
Bianchi, S.
Bisnovatvi-Kogan, G.
Blasi, P.
Blay, P.
Bodaghee, A.
Boer, M.
Boettcher, M.
Bogdanov, S.
Bombaci, I
Bonino, R.
Braga, J.
Brandt, W.
Brez, A.
Bucciantini, N.
Burderi, L.
Caiazzo, I
Campana, R.
Campana, S.
Capitanio, F.
Cappi, M.
Cardillo, M.
Casella, P.
Catmabacak, O.
Cenko, B.
Cerda-Duran, P.
Cerruti, C.
Chaty, S.
Chauvin, M.
Chen, V
Chenevez, J.
Chernyakova, M.
Teddy, Cheung C. C.
Christodoulou, D.
Connell, P.
Corbet, R.
Zelati, Coti F.
Covino, S.
Cui, W.
Cusumano, G.
D'Ai, A.
D'Ammando, F.
Dadina, M.
De Rosa, A.
De Ruvo, L.
Degenaar, N.
Del Santo, M.
Del Zanna, L.
Dewangan, G.
Di Cosimo, S.
Di Lalla, N.
Di Persio, G.
Di Salvo, T.
Dias, T.
Done, C.
Dovciak, M.
Doyle, G.
Ducci, L.
Elsner, R.
Enoto, T.
Escada, J.
Esposito, P.
Eyles, C.
Fabiani, S.
Falanga, M.
Falocco, S.
Fan, Y.
Fender, R.
Feroci, M.
Ferrigno, C.
Forman, W.
Foschini, L.
Fragile, C.
Fuerst, F.
Fujita, Y.
Gasent-Blesa, J. L.
Gelfand, J.
Gendre, B.
Ghirlanda, G.
Ghisellini, G.
Giroletti, M.
Goetz, D.
Gomez, J. -L
Gonzalez, D.
Gonzalcz-Riestra, R.
Gotthelf, E.
Gou, L.
Grandi, P.
Grinberg, V
Grise, F.
Guidorzi, C.
Gurlebeck, N.
Guver, T.
Haggard, D.
Hardcastle, M.
Hartmann, D.
Haswell, C.
Heger, A.
Hernanz, M.
Heyl, J.
Ho, L.
Hoormann, J.
Horak, J.
Huovelin, J.
Huppenkothen, D.
Iaria, R.
Inam, Sitki C.
Ingram, A.
Israel, G.
Izzo, L.
Burgess, M.
Jackson, M.
Ji, L.
Ji, L.
Jiang, J.
Johannsen, T.
Jones, C.
Jorstad, S.
Kajava, J. J. E.
Kalamkar, M.
Kalemci, L.
Kallman, T.
Kamble, A.
Kislat, F.
Kiss, M.
Klochkov, D.
Koerding, E.
Kolehmainen, M.
Koljonen, K.
Komossa, S.
Kong, A.
Korpela, S.
Kowalinski, M.
Krawczynski, H.
Kreykenbohm, I
Kuss, M.
Lai, D.
Lan, M.
Larsson, J.
Laycock, S.
Lazzati, D.
Leahy, D.
Li, H.
Li, J.
Li, L. -X
Li, T.
Li, Z.
Linares, M.
Lister, M.
Liu, H.
Lodato, G.
Lohfink, A.
Longo, F.
Luna, G.
Lutovinov, A.
Mahmoodifar, S.
Maia, J.
Mainieri, V
Maitra, C.
Maitra, D.
Majczyna, A.
Maldera, S.
Malyshev, D.
Manfreda, A.
Manousakis, A.
Manuel, R.
Margutti, R.
Marinucci, A.
Markoff, S.
Marschcr, A.
Marshall, H.
Massaro, F.
McLaughlin, M.
Medina-Tanco, G.
Mehdipour, N.
Middleton, N.
Mignari, R.
Mimica, P.
Mineo, T.
Mingo, B.
Miniutti, G.
Mirac, S. M.
Morlino, G.
Motlagli, A., V
Motta, S. E.
Muslitukov, A.
Nagataki, S.
Nardini, F.
Nattila, J.
Navarro, G. J.
Negri, B.
Negro, M.
Nenonen, S.
Neustroev, V
Nicastro, F.
Norton, A.
Nucita, A.
O'Brien, P.
O'Dell, S.
Odaka, H.
Olmi, B.
Omodei, N.
Orienti, M.
Orlandini, M.
Osborne, J.
Pacciani, L.
Paliya, V. S.
Papadakis, I
Papitto, A.
Paragi, Z.
Pascal, P.
Paul, B.
Pavan, L.
Pellizzoni, A.
Perinati, E.
Pesce-Rollins, M.
Piconcelli, E.
Pili, A. G.
Pilia, M.
Pohl, M.
Ponti, G.
Porquet, D.
Possenti, A.
Postnov, K.
Prandoni, I
Produit, N.
Puehlhofer, G.
Ramsey, B.
Razzano, M.
Rea, N.
Reig, P.
Reinsch, K.
Reiprich, T.
Reynolds, M.
Risaliti, G.
Roberts, T.
Rodriguez, J.
Rossi, M. E.
Rosswog, S.
Rozanska, A.
Rubini, A.
Rudak, B.
Russell, D.
Ryde, F.
Sabatini, S.
Sala, G.
Salvati, M.
Sasaki, M.
Savolainen, T.
Saxton, R.
Scaringi, S.
Schawinski, K.
Schulz, N. S.
Schwope, A.
Severgnini, P.
Sharon, M.
Shaw, A.
Shearer, A.
Shesheng, X.
Shih, I. -C
Silva, K.
Silva, R.
Silver, E.
Sniale, A.
Spada, F.
Spandre, G.
Stamerra, A.
Stappers, B.
Starrfield, S.
Stawarz, L.
Stergioulas, N.
Stevens, A.
Stiele, H.
Suleimanov, V
Sunyaev, R.
Slowikowska, A.
Tamborra, F.
Tavecchio, F.
Taverna, R.
Tiengo, A.
Tolos, L.
Tombesi, F.
Tomsick, J.
Tong, H.
Torok, G.
Torres, D. F.
Tortosa, A.
Tramacere, A.
Trimble, V
Trinchieri, G.
Tsygankov, S.
Tuerler, M.
Turriziani, S.
Ursini, F.
Uttley, P.
Varniere, P.
Vincent, F.
Vurgun, E.
Wang, C.
Wang, Z.
Watts, A.
Wheeler, J. C.
Wiersema, K.
Wijnands, R.
Wilms, J.
Wolter, A.
Wood, K.
Wu, K.
Wu, X.
Xiangyu, W.
Xie, F.
Xu, R.
Yan, S. -P
Yang, J.
Yu, W.
Yuan, F.
Zajczyk, A.
Zanetti, D.
Zanin, R.
Zanni, C.
Zappacosta, L.
Zdziarski, A. A.
Zech, A.
Zhang, H.
Zhang, S.
Zhang, S.
Zhang, W.
Zoghbi, A.
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI XIPE the X-ray Imaging Polarimetry Explorer
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray Astronomy; Polarimetry; X-ray optics; Gas Pixel Detector
ID GAS PIXEL DETECTOR; POLARIZATION; RADIATION
AB XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially- resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X- ray astronomers with 75% of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.
C1 [Soffitta, P.; Costa, E.; Muleri, F.; Attina, P.; Del Monte, E.; Donnarunnna, I; Evangelista, Y.; Capitanio, F.; Cardillo, M.; De Rosa, A.; Di Cosimo, S.; Di Persio, G.; Fabiani, S.; Feroci, M.; Pacciani, L.; Rubini, A.; Sabatini, S.] IAPS INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
[Bellazzini, R.; Baldini, L.; Minuti, M.; Pinchera, M.; Sgro, C.; Bombaci, I; Brez, A.; De Ruvo, L.; Di Lalla, N.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Spada, F.; Spandre, G.; Zanetti, D.] Univ Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
[Bellazzini, R.; Baldini, L.; Minuti, M.; Pinchera, M.; Sgro, C.; Bombaci, I; Brez, A.; De Ruvo, L.; Di Lalla, N.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Spada, F.; Spandre, G.; Zanetti, D.] INFN Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
[Bozzo, E.; Courvoisier, T.; Paltani, S.; Ducci, L.; Ferrigno, C.; Malyshev, D.; Pavan, L.; Produit, N.; Tramacere, A.; Tuerler, M.] Univ Geneva, Dept Astron, Chemin Ecogia 16, CH-1290 Versoix, Switzerland.
[Burwitz, V; Nandra, K.; Backer, W.; Ponti, G.; Scaringi, S.] MPI Fuer Extraterrestr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Castro-Tirado, A. J.; Gomez, J. -L; Hernanz, M.; Li, J.; Rea, N.; Tolos, L.; Torres, D. F.] CSIC, Inst Astrofs Andaluca, Apt 3004, E-18080 Granada, Spain.
[Feng, H.; Li, H.; Li, T.] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China.
[Feng, H.; Li, H.; Li, T.] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China.
[Feng, H.] Tsinghua Univ, Minist Educ, Key Lab Particle & Radiat Imaging, Haidian Qu, Beijing Shi, Peoples R China.
[Gburek, S.; Kowalinski, M.] Polish Acad Sci, Solar Phys Div, Space Res Ctr, PL-51622 Wroclaw, Poland.
[Goosmann, R.; Grosso, N.; Grise, F.; Porquet, D.] Observ Astron, 11 Rue Luniv, F-67000 Strasbourg, France.
[Karas, V; Marin, F.; Svoboda, J.; Dovciak, M.; Horak, J.] Astron Inst Acad Sci Czech Republ, Bocni II 1401, CZ-14131 Prague, Czech Republic.
[Matt, G.; Bianchi, S.; Marinucci, A.; Tamborra, F.; Tortosa, A.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
[Poutanen, J.; Neustroev, V] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Maria, Sabau D.; Manuel, R.; Miniutti, G.] Natl Inst Aerosp Technol INTA, Carretera Ajalvir Km 4, Torrejon De Ardoz 28850, Spain.
[Santangelo, A.; Tenzer, C.; Doroslienko, V; Ducci, L.; Klochkov, D.; Perinati, E.; Puehlhofer, G.; Sasaki, M.; Suleimanov, V] IAAT Univ Tuebingen, Sand 1, D-72076 Tubingen, Germany.
[Tagliaferri, G.; Pareschi, G.; Spiga, D.; Ballo, L.; Basso, S.; Campana, S.; Zelati, Coti F.; Covino, S.; Foschini, L.; Ghirlanda, G.; Ghisellini, G.; Guidorzi, C.; Severgnini, P.; Tavecchio, F.; Trinchieri, G.; Wolter, A.] INAF OA Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy.
[Reglero, V; Macian, J.; Pinazo, H. B.; Rodriguez, J. P.; Blay, P.; Cerda-Duran, P.; Cerruti, C.; Connell, P.; Eyles, C.; Gasent-Blesa, J. L.; Mimica, P.; Navarro, G. J.] Univ Valencia, Av de Vicente Blasco Ibez 13, Valencia 46010, Spain.
[Weisskopf, M. C.; Cenko, B.; Elsner, R.; O'Dell, S.; Ramsey, B.] NASA, Marshall Space Flight Control Ctr, Washington, DC USA.
[Zane, S.; Theobald, C.; Theodorou, T.; Winter, B.; Gonzalez, D.; Wu, X.] MSSL, Dorking RH5 6NT, Surrey, England.
[Agudo, I] Glorieta Astronoma IAAC CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Bykov, A.] Ioffe Physicotech Inst, Politekhn Skaya 26, St Petersburg 194021, Russia.
[Churazov, E.; Sunyaev, R.; Zhang, W.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1317, D-85711 Garching, Germany.
[De Martino, D.] INAF OA Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy.
[Gallo, E.; Zoghbi, A.] Univ Michigan Astron, 1085 S Univ Ave,305A West Hall, Ann Arbor, MI 48109 USA.
[Kaaret, P.; Reynolds, M.] Michigan State Univ, 567 Wilson Rd, E Lansing, MI 48824 USA.
[Malzac, J.; Atteia, J. -L; Belmont, R.] IRAP, Ave Colonel Roche,9,BP, F-44346 Toulouse, France.
[Doyle, G.] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
[Mundell, C.] Univ Bath, Claverton Down, Bath BA2 7AY, Avon, England.
[Perna, R.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Petrucci, P. -O; Ursini, F.] Univ Grenoble Alpes, Inst Planetol & Astrophys Grenoble, CS 40700, F-38058 Grenoble 9, France.
[Roncadelli, M.] INFN Pavia, Via Agostino Bassi 6, I-27100 Pavia, Italy.
[Sazonov, S.; Bisnovatvi-Kogan, G.; Lutovinov, A.] Russian Acad Sci, Space Res Inst, 84-32 Profsoyuznaya Str, Moscow, Russia.
[Turolla, R.; Taverna, R.] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy.
[Vink, J.; Altamirano, D.; Degenaar, N.; Ingram, A.; Markoff, S.; Muslitukov, A.; Stevens, A.; Uttley, P.; Watts, A.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[de Ona, Wilhelmi E.] Inst Ciences Espai, Campus UAB,Carrer Can Magrans S-N, Cerdanyola Del Valles 08193, Spain.
[Ferreira, I; Kuulkers, E.; Laranaga, J.; Lumb, D. H.; Oosterbroek, T.; Santovincenzo, A.] ESA ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Akbar, A. M.] Effat Univ, POB 34689, Jeddah 21478, Saudi Arabia.
[Allan, H.; Chenevez, J.] Tech Univ Denmark, Natl Space Inst, Elektrovej Bld 327, DK-2800 Lyngby, Denmark.
[Aloisio, B.; Amato, E.; Bandiera, R.; Blasi, P.; Bucciantini, N.; Del Zanna, L.; Risaliti, G.; Salvati, M.] INAF, Arcetri Observ, Largo Enrico Fermi 5, I-50125 Florence, Italy.
[Amati, L.; Campana, R.; Cappi, M.; D'Ammando, F.; Dadina, M.; Giroletti, M.; Grandi, P.; Orienti, M.; Orlandini, M.] INAF IASF Bologna, Via P Gobetti 101, I-40129 Bologna, Italy.
[Angelakis, E.; Komossa, S.] Max Planck Inst Radioastron, Auf Hgel 69, D-53121 Bonn, Endenich, Germany.
[Antonelli, A.] ASDC, Via Politecn Snc, I-00133 Rome, Italy.
[Arezu, J.] Buein Zahra Tech Univ, Dept Phys & Engn Phys, Qazvin, Iran.
[Pearce, M.; Axelsson, M.; Chauvin, M.; Burgess, M.; Kiss, M.; Larsson, J.; Ryde, F.; Xie, F.] KTH Royal Inst Technol, Valhallavagen 79, S-10044 Stockholm, Sweden.
[Bachetti, M.; Pellizzoni, A.; Pilia, M.; Possenti, A.] INAF OA Cagliari, Str 54, I-09012 Capoterra, Italy.
[Latronico, L.; Bonino, R.; Maldera, S.; Manfreda, A.; Massaro, F.; Negro, M.] INFN Torino, Via Pietro Giuria 1, I-10125 Turin, Italy.
[Balman, S.; Baykal, Altan; Inam, Sitki C.; Mirac, S. M.] Middle East Tech Univ, Mah Dumlupnar Blv 1, TR-06800 Ankara, Turkey.
[Barcons, N.] Inst Fsica Cantabria, E-39005 Santander, Spain.
[Behar, E.] Technion Israel Inst Technol, IL-3200003 Haifa, Israel.
[Beheshtipour, B.; Hoormann, J.; Kislat, F.; Krawczynski, H.; Zajczyk, A.] Washington Univ, 1 Brookings Dr, St Louis, MO 63130 USA.
[Berger, L.; Forman, W.; Jones, C.; Kamble, A.; Silver, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bernardini, F.; Gelfand, J.; Huppenkothen, D.; Koljonen, K.; Russell, D.] NYUAD, POB 129188, Abu Dhabi, U Arab Emirates.
[Bodaghee, A.] Georgia Coll, 231 W Hancock St, Milledgeville, GA 31061 USA.
[Boer, M.] Univ Nice Sophia Antipolis, CNRS, ARTEMIS UMR 7250, Observ Cote Azur,CS 34229, F-06304 Nice, France.
[Boettcher, M.] North West Univ, Albert Luthuli & Univ Dr, ZA-2790 Mmabatho, Mahikeng, South Africa.
[Bogdanov, S.; Gotthelf, E.] Columbia Univ, 116th St & Broadway, New York, NY 10027 USA.
[Braga, J.; Silva, K.] INPE, Ave Astronautas 1-758,Jd Granja, BR-12227010 Sao Jose Dos Campos, Brazil.
[Brandt, W.] Penn State Univ, University Pk, PA 16802 USA.
[Burderi, L.] Univ Cagliari, Str Prov Sestu KM 1, I-09042 Monserrato, Italy.
[Caiazzo, I; Heyl, J.] Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Carpentiero, R.; Cavazzuti, E.; Negri, B.] Agenzia Spaziale Italiana, Unita Osservaz Universo, Viale Liegi 26, I-00198 Rome, Italy.
[Casella, P.; Israel, G.; Kalamkar, M.; Nicastro, F.; Papitto, A.; Piconcelli, E.; Prandoni, I; Zappacosta, L.] INAF OA Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Catmabacak, O.; Kalemci, L.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Chaty, S.; Goetz, D.; Maitra, C.; Rodriguez, J.] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France.
[Chen, V; Lan, M.; Wu, K.; Xiangyu, W.] Nanjing Univ, 22 Hankou Rd, Nanjing 210093, Jiangsu, Peoples R China.
[Chernyakova, M.] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland.
[Teddy, Cheung C. C.; Wood, K.] NRL, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Christodoulou, D.; Laycock, S.; Yang, J.] Univ Massachusetts, 1 Univ Ave, Lowell, MA 01852 USA.
[Corbet, R.] Univ Maryland, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Cui, W.; Lister, M.] Purdue Univ, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
[Cusumano, G.; Del Santo, M.; Mineo, T.] INAF IASF, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[D'Ai, A.; Di Salvo, T.; Iaria, R.] Univ Palermo, Dipartimento Fis, Via Archirafi 36, I-90123 Palermo, Italy.
[Dewangan, G.; Dias, T.] Interuniv Ctr Astron & Astrophys, Pune Univ Campus, Pune 411007, Maharashtra, India.
[Escada, J.; Maia, J.; Silva, R.] Univ Coimbra, Dept Fsica, LIP, P-3004516 Coimbra, Portugal.
[Done, C.; Kolehmainen, M.; Roberts, T.] Univ Durham, Stockton Rd, Durham DH1 3UP, England.
[Enoto, T.; Kallman, T.; Mahmoodifar, S.; Sniale, A.] Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Esposito, P.; Mignari, R.] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy.
[Falanga, M.] ISSI, Hallerstr 6, CH-3012 Bern, Switzerland.
[Falocco, S.] Univ Napoli Federico II, Dipartimento Fis, Via Cinthia, I-80126 Naples, Italy.
[Fan, Y.; Ji, L.; Yan, S. -P] Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China.
[Fender, R.; Motta, S. E.] Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
[Fragile, C.] Coll Charleston, 66 George St, Charleston, SC 29424 USA.
[Fuerst, F.] CALTECH, MC 290-17, Pasadena, CA 91125 USA.
[Fujita, Y.] Osaka Univ, 1-1 Machikaneyama Cho, Toyonaka, Osaka 5600043, Japan.
[Gendre, B.] Univ Virgin Isl, Coll Sci, 2 John Brewers Bay, St Thomas, VI 00802 USA.
[Gonzalcz-Riestra, R.] VILSPA, ESA, XMM Newton Sci Operat Ctr, POB 50727, E-28080 Madrid, Spain.
[Gou, L.; Wang, C.] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing, Peoples R China.
[Grinberg, V; Linares, M.; Marshall, H.; Schulz, N. S.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Gurlebeck, N.] Univ Bremen, Ctr Appl Space Technol & Micrograv, ZARM, D-28359 Bremen, Germany.
[Guver, T.; Motlagli, A., V; Vurgun, E.] Istanbul Univ, TR-34452 Beyazit, Fatih Stanbul, Turkey.
[Haggard, D.] McGill Univ, 3550 Univ St, Montreal, PQ H3A 2A7, Canada.
[Ness, J. U.; Kajava, J. J. E.; Saxton, R.] ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain.
[Hardcastle, M.] Univ Hertfordshire, De Havilland Campus, Hatfield AL10 9EU, Herts, England.
[Hartmann, D.; Paliya, V. S.] Clemson Univ, Clemson, SC 29634 USA.
[Haswell, C.; Norton, A.] Open Univ, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Heger, A.; Ho, L.] Monash Univ, Sch Phys, Monash Ctr Astrophys, Clayton, Vic 3800, Australia.
[Heger, A.; Ho, L.] Monash Univ, Sch Math Sci, Clayton, Vic 3800, Australia.
[Xu, R.] Peking Univ, 5 Yiheyuan Rd Haidian Dist, Beijing 100871, Peoples R China.
[Stiele, H.] Tsinghua Univ, 30 Shuangqing Rd, Beijing, Peoples R China.
[Huovelin, J.; Korpela, S.] Univ Helsinki, Dept Phys, Div Geophys & Astron, POB 48, FI-00014 Helsinki, Finland.
[Izzo, L.] Sapienza Univ, Ple A Moro 2, I-00185 Rome, Italy.
[Izzo, L.] ICRA, Ple A Moro 2, I-00185 Rome, Italy.
[Jackson, M.] Cardiff Univ, Cardiff CF10 3XQ, Wales.
[Jiang, J.] Fudan Univ, 220 Handan Rd, Shanghai, Peoples R China.
[Ji, L.; Zhang, S.; Zhang, S.] Inst High Energy Phys, 19B YuquanLu, Beijing 1000049, Peoples R China.
[Johannsen, T.] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada.
[Jorstad, S.] Boston Univ, Inst Astrophys Res, Address 725 Commonwealth Ave, Boston, MA 02215 USA.
[Koerding, E.] Radboud Univ Nijmegen, Comeniuslaan 4, NL-6525 HP Nijmegen, Netherlands.
[Kong, A.] Natl Tsing Hua Univ, 101,Sect 2,Guangiu Rd, Hsinchu, Taiwan.
[Kreykenbohm, I; Wilms, J.] Univ Erlangen Nurnberg, Schlosspl 4, D-91054 Erlangen, Germany.
[Lai, D.] Cornell Univ, Space Bldg, Ithaca, NY 14853 USA.
[Lazzati, D.] Oregon State Univ, Dept Phys, 301 Weniger Hall, Corvallis, OR 97331 USA.
[Leahy, D.] Univ Calgary, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
[Li, L. -X] Kavli Inst Astron & Astrophys, Qinghua W Rd, Beijing, Peoples R China.
[Li, Z.] Xiangtan Univ, Dept Phys, Xiangtan, Hunan, Peoples R China.
[Liu, H.] Guangxi Univ, Nanning, Xixiangtang, Peoples R China.
[Lodato, G.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.
[Lohfink, A.; Middleton, N.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Longo, F.] Univ Trieste, Via Alfonso Valerio 32, I-34128 Trieste, Italy.
[Luna, G.] IAFE COBNICET, RA-2290 Buenos Aires, DF, Argentina.
[Mainieri, V] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Maitra, D.] Wheaton Coll, Dept Phys & Astron, 501 Coll Ave, Wheaton, IL 60187 USA.
[Majczyna, A.] Natl Ctr Nucl Res, Andrzeja Soltana 7, PL-05400 Otwock, Poland.
[Manousakis, A.; Rozanska, A.; Rudak, B.; Zdziarski, A. A.] Copernicus Astron Ctr, Bartycka 18, Warsaw, Poland.
[Margutti, R.] NYU, New York, NY USA.
[Marschcr, A.] Boston Univ, Boston, MA 02215 USA.
[Massaro, E.; Shesheng, X.] Univ Roma La Sapienza, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
[McLaughlin, M.] West Virginia Univ, Morgantown, WV 26506 USA.
[Medina-Tanco, G.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Apartado Postal 70-543,Ciudad Univ, Mexico City 04510, DF, Mexico.
[Mehdipour, N.] SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Mingo, B.; O'Brien, P.; Osborne, J.; Wiersema, K.] Univ Leicester, Univ Rd, Leicester LE1 7RH, Leics, England.
[Morlino, G.] Gran Sasso Sci Inst, Viale Francesco Crispi 7, Laquila, Italy.
[Nagataki, S.] RIKEN, Wako, Saitama, Japan.
[Nardini, F.] Keele Univ, Keele ST5 5BG, Staffs, England.
[Nattila, J.; Tsygankov, S.] Tuorla Observ, Vaisalantie 20, Piikkio 21500, Finland.
[Nenonen, S.] Oxford Instruments Analyt Oy, Tarvonsalmenkatu 17, Espoo, Finland.
[Nucita, A.] Univ Lecce, Piazza Tancredi N7, I-73100 Lecce, Italy.
[Odaka, H.] ISAS JAXA, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Olmi, B.; Pili, A. G.] Univ Florence, Piazza San Marco 4, I-50121 Florence, Italy.
[Omodei, N.] Kipac, 2575 Sand Hill Rd,M-S 29, Menlo Pk, CA 94025 USA.
[Pohl, M.] Univ Geneva, DPNC, Quai Ernest Ansermet 30, CH-1205 Geneva, Switzerland.
[Papadakis, I] Univ Crete, Phys Dept, GR-71003 Iraklion, Greece.
[Paragi, Z.] Joint Inst VLBI Europe JIVE, Postbus 2, NL-7090 AA Dwingeloo, Netherlands.
[Pascal, P.] Observ Midi Pyrenees, 14 Ave Edouard Belim, F-31400 Toulouse, France.
[Paul, B.] Raman Res Inst, C V Raman Ave, Sadashivanagar 560080, India.
[Postnov, K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Reig, P.] Fdn Res & Technol Hellas, Leof Plastira 100, Iraklion 70013, Greece.
[Reinsch, K.] Georg August Univ Goettingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
[Reiprich, T.] Argelander Inst Astron, Auf Hugel 71, D-53121 Bonn, Germany.
[Rossi, M. E.] Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Rosswog, S.] Stockholm Univ, Univ Vagen 10, S-11418 Stockholm, Sweden.
[Sala, G.] Univ Politecn Cataluna, Campus Nord,Calle Jordi Girona 1-3, Barcelona 08034, Spain.
[Savolainen, T.] Aalto Univ, Metsahovi Radio Observ, POB 13000, FI-00076 Aalto, Finland.
[Schawinski, K.] Swiss Fed Inst Technol, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Schwope, A.] Leibniz Inst Astrophys Potsdam, An Sternwarte 16, D-14482 Potsdam, Germany.
[Sharon, M.] Univ Alberta, Edmonton, AB T6G 2E9, Canada.
[Shaw, A.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Shearer, A.] Natl Univ Ireland Galway, Univ Rd, Galway, Ireland.
[Shih, I. -C; Vincent, F.; Zech, A.] Observ Paris, 61 Ave Observ, F-75014 Paris, France.
[Stamerra, A.; Zanni, C.] INAF OA Torino, I-10024 Turin, Italy.
[Stappers, B.] Univ Manchester, Booth St West, Manchester M15 6PB, Lancs, England.
[Starrfield, S.] Arizona State Univ Tempe, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, Ft 38 Skala,Orla 171, PL-30244 Krakow, Poland.
[Stergioulas, N.] Aristotle Univ Thessaloniki, Thessaloniki 54124, Greece.
[Slowikowska, A.] Janusz Gil Inst Astron, Ul Szafrana 2, PL-65516 Zielona Gora, Poland.
[Tiengo, A.] Ist Univ Super Pavia, IUSS, Palazzo Broletto,Piazza Vittoria 15, I-27100 Pavia, Italy.
[Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Tong, H.] Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China.
[Torok, G.] Silesian Univ Opava, Na Rybnicku 626-1, Opava 74601, Czech Republic.
[Trimble, V] Univ Calif Irvine, Phys Astron Dept, Phys 4575, Irvine, CA 92697 USA.
[Turriziani, S.] Univ Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy.
[Varniere, P.] Univ Paris Diderot, AstroParticule & Cosmol, APC, CNRS,UMR 7164,N2P3, F-75205 Paris 13, France.
[Wang, Z.] Tongji Univ, Shanghai 200092, Peoples R China.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA.
[Yu, W.; Yuan, F.] Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China.
[Zanin, R.] Tech Univ Darmstadt, Inst Kernphys, D-64289 Darmstadt, Germany.
[Zhang, H.] Los Alamos Natl Lab, Theoret Div, Los Alamos, NM 87545 USA.
RP Soffitta, P (reprint author), IAPS INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
RI Bykov, Andrei/E-3131-2014; Miniutti, Giovanni/L-2721-2014; Karas,
Vladimir/C-1559-2013; Horak, Jiri/G-9015-2014; Svoboda,
Jiri/G-9045-2014; Dovciak, Michal/F-4258-2014; Marin,
Frederic/A-3737-2015;
OI Poutanen, Juri/0000-0002-0983-0049; Blasi, Pasquale/0000-0003-2480-599X;
Miniutti, Giovanni/0000-0003-0707-4531; Karas,
Vladimir/0000-0002-5760-0459; Dovciak, Michal/0000-0003-0079-1239; de
Martino, Domitilla/0000-0002-5069-4202; Gendre,
Bruce/0000-0002-9077-2025; orienti, monica/0000-0003-4470-7094; Del
Zanna, Luca/0000-0001-5200-882X; Angelakis,
Emmanouil/0000-0001-7327-5441
NR 25
TC 1
Z9 1
U1 10
U2 10
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 990515
DI 10.1117/12.2233046
PN 1
PG 20
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500030
ER
PT S
AU Takahashi, T
Kokubun, M
Mitsuda, K
Kelley, R
Ohashi, T
Aharonian, F
Akamatsu, H
Akimoto, F
Allen, S
Anabuki, N
Angelini, L
Arnaud, K
Asai, M
Audard, M
Awaki, H
Axelsson, M
Azzarello, P
Baluta, C
Bamba, A
Bando, N
Bautz, M
Bialas, T
Blandford, R
Boyce, K
Brenneman, L
Brown, G
Bulbul, E
Cackett, E
Canavan, E
Chernyakova, M
Chiao, M
Coppi, P
Costantini, E
de Plaa, J
den Herder, JW
DiPirro, M
Done, C
Dotani, T
Doty, J
Ebisawa, K
Eckart, M
Enoto, T
Ezoe, Y
Fabian, A
Ferrigno, C
Foster, A
Fujimoto, R
Fukazawa, Y
Furuzawa, A
Galeazzi, M
Gallo, L
Gandhi, P
Gilmore, K
Giustini, M
Goldwurm, A
Gu, LY
Guainazzi, M
Haas, D
Haba, Y
Hagino, K
Hamaguchi, K
Harayama, A
Harrus, I
Hatsukade, I
Hayashi, T
Hayashi, K
Hayashida, K
Hiraga, J
Hirose, K
Hornschemeier, A
Hoshino, A
Hughes, J
Ichinohe, Y
Iizuka, R
Inoue, Y
Inoue, H
Ishibashi, K
Ishida, M
Ishikawa, K
Ishimura, K
Ishisaki, Y
Itoh, M
Iwata, N
Iyomoto, N
Jewell, C
Kaastra, J
Kallman, T
Kamae, T
Kara, E
Kataoka, J
Katsuda, S
Katsuta, J
Kawaharada, M
Kawai, N
Kawano, T
Kawasaki, S
Khangulyan, D
Kilbourne, C
Kimball, M
King, A
Kitaguchi, T
Kitamoto, S
Kitayama, T
Kohmura, T
Kosaka, T
Koujelev, A
Koyama, K
Koyama, S
Kretschmar, P
Krimm, H
Kubota, A
Kunieda, H
Laurent, P
Lebrun, F
Lee, SH
Leutenegger, M
Limousin, O
Loewenstein, M
Long, K
Lumb, D
Madejski, G
Maeda, Y
Maier, D
Makishima, K
Markevitch, M
Masters, C
Matsumoto, H
Matsushita, K
McCammon, D
Mcguinness, D
McNamara, B
Mehdipour, M
Miko, J
Miller, J
Miller, E
Mineshige, S
Minesugi, K
Mitsuishi, I
Miyazawa, T
Mizuno, T
Mori, K
Mori, H
Moroso, F
Moseley, H
Muench, T
Mukai, K
Murakami, H
Murakami, T
Mushotzky, R
Nagano, H
Nagino, R
Nakagawa, T
Nakajima, H
Nakamori, T
Nakano, T
Nakashima, S
Nakazawa, K
Namba, Y
Natsukari, C
Nishioka, Y
Nobukawa, M
Nobukawa, K
Noda, H
Nomachi, M
O' Dell, S
Odaka, H
Ogawa, H
Ogawa, M
Ogi, K
Ohno, M
Ohta, M
Okajima, T
Okamoto, A
Okazaki, T
Ota, N
Ozaki, M
Paerels, F
Paltani, S
Parmar, A
Petre, R
Pinto, C
Pohl, M
Pontius, J
Porter, FS
Pottschmidt, K
Ramsey, B
Reynolds, C
Russell, H
Safi-Harb, S
Saito, S
Sakai, S
Sakai, K
Sameshima, H
Sasaki, T
Sato, G
Sato, Y
Sato, K
Sato, R
Sawada, M
Schartel, N
Serlemitsos, P
Seta, H
Shibano, Y
Shida, M
Shidatsu, M
Shimada, T
Shinozaki, K
Shirron, P
Simionescu, A
Simmons, C
Smith, R
Sneiderman, G
Soong, Y
Stawarz, L
Sugawara, Y
Sugita, H
Sugita, S
Szymkowiak, A
Tajima, H
Takahashi, H
Takeda, S
Takei, Y
Tamagawa, T
Tamura, T
Tamura, K
Tanaka, T
Tanaka, Y
Tanaka, Y
Tashiro, M
Tawara, Y
Terada, Y
Terashima, Y
Tombesi, F
Tomida, H
Tsuboi, Y
Tsujimoto, M
Tsunemi, H
Tsuru, T
Uchida, H
Uchiyama, Y
Uchiyama, H
Ueda, Y
Ueda, S
Ueno, S
Uno, S
Urry, M
Ursino, E
de Vries, C
Wada, A
Watanabe, S
Watanabe, T
Werner, N
Wik, D
Wilkins, D
Williams, B
Yamada, T
Yamada, S
Yamaguchi, H
Yamaoka, K
Yamasaki, N
Yamauchi, M
Yamauchi, S
Yaqoob, T
Yatsu, Y
Yonetoku, D
Yoshida, A
Yuasa, T
Zhuravleva, I
Zoghbi, A
AF Takahashi, Tadayuki
Kokubun, Motohide
Mitsuda, Kazuhisa
Kelley, Richard
Ohashi, Takaya
Aharonian, Felix
Akamatsu, Hiroki
Akimoto, Fumie
Allen, Steve
Anabuki, Naohisa
Angelini, Lorella
Arnaud, Keith
Asai, Makoto
Audard, Marc
Awaki, Hisamitsu
Axelsson, Magnus
Azzarello, Philipp
Baluta, Chris
Bamba, Aya
Bando, Nobutaka
Bautz, Marshall
Bialas, Thomas
Blandford, Roger
Boyce, Kevin
Brenneman, Laura
Brown, Greg
Bulbul, Esra
Cackett, Edward
Canavan, Edgar
Chernyakova, Maria
Chiao, Meng
Coppi, Paolo
Costantini, Elisa
de Plaa, Jelle
den Herder, Jan-Willem
DiPirro, Michael
Done, Chris
Dotani, Tadayasu
Doty, John
Ebisawa, Ken
Eckart, Megan
Enoto, Teruaki
Ezoe, Yuichiro
Fabian, Andrew
Ferrigno, Carlo
Foster, Adam
Fujimoto, Ryuichi
Fukazawa, Yasushi
Furuzawa, Akihiro
Galeazzi, Massimiliano
Gallo, Luigi
Gandhi, Poshak
Gilmore, Kirk
Giustini, Margherita
Goldwurm, Andrea
Gu, Liyi
Guainazzi, Matteo
Haas, Daniel
Haba, Yoshito
Hagino, Kouichi
Hamaguchi, Kenji
Harayama, Atsushi
Harrus, Ilana
Hatsukade, Isamu
Hayashi, Takayuki
Hayashi, Katsuhiro
Hayashida, Kiyoshi
Hiraga, Junko
Hirose, Kazuyuki
Hornschemeier, Ann
Hoshino, Akio
Hughes, John
Ichinohe, Yuto
Iizuka, Ryo
Inoue, Yoshiyuki
Inoue, Hajime
Ishibashi, Kazunori
Ishida, Manabu
Ishikawa, Kumi
Ishimura, Kosei
Ishisaki, Yoshitaka
Itoh, Masayuki
Iwata, Naoko
Iyomoto, Naoko
Jewell, Chris
Kaastra, Jelle
Kallman, Timothy
Kamae, Tuneyoshi
Kara, Erin
Kataoka, Jun
Katsuda, Satoru
Katsuta, Junichiro
Kawaharada, Madoka
Kawai, Nobuyuki
Kawano, Taro
Kawasaki, Shigeo
Khangulyan, Dmitry
Kilbourne, Caroline
Kimball, Mark
King, Ashley
Kitaguchi, Takao
Kitamoto, Shunji
Kitayama, Tetsu
Kohmura, Takayoshi
Kosaka, Tatsuro
Koujelev, Alex
Koyama, Katsuji
Koyama, Shu
Kretschmar, Peter
Krimm, Hans
Kubota, Aya
Kunieda, Hideyo
Laurent, Philippe
Lebrun, Francois
Lee, Shiu-Hang
Leutenegger, Maurice
Limousin, Olivier
Loewenstein, Michael
Long, Knox
Lumb, David
Madejski, Grzegorz
Maeda, Yoshitomo
Maier, Daniel
Makishima, Kazuo
Markevitch, Maxim
Masters, Candace
Matsumoto, Hironori
Matsushita, Kyoko
McCammon, Dan
Mcguinness, Daniel
McNamara, Brian
Mehdipour, Missagh
Miko, Joseph
Miller, Jon
Miller, Eric
Mineshige, Shin
Minesugi, Kenji
Mitsuishi, Ikuyuki
Miyazawa, Takuya
Mizuno, Tsunefumi
Mori, Koji
Mori, Hideyuki
Moroso, Franco
Moseley, Harvey
Muench, Theodore
Mukai, Koji
Murakami, Hiroshi
Murakami, Toshio
Mushotzky, Richard
Nagano, Housei
Nagino, Ryo
Nakagawa, Takao
Nakajima, Hiroshi
Nakamori, Takeshi
Nakano, Toshio
Nakashima, Shinya
Nakazawa, Kazuhiro
Namba, Yoshiharu
Natsukari, Chikara
Nishioka, Yusuke
Nobukawa, Masayoshi
Nobukawa, Kumiko
Noda, Hirofumi
Nomachi, Masaharu
O' Dell, Steve
Odaka, Hirokazu
Ogawa, Hiroyuki
Ogawa, Mina
Ogi, Keiji
Ohno, Masanori
Ohta, Masayuki
Okajima, Takashi
Okamoto, Atsushi
Okazaki, Tsuyoshi
Ota, Naomi
Ozaki, Masanobu
Paerels, Frits
Paltani, Stephane
Parmar, Arvind
Petre, Robert
Pinto, Ciro
Pohl, Martin
Pontius, James
Porter, F. Scott
Pottschmidt, Katja
Ramsey, Brian
Reynolds, Christopher
Russell, Helen
Safi-Harb, Samar
Saito, Shinya
Sakai, Shin-ichiro
Sakai, Kazuhiro
Sameshima, Hiroaki
Sasaki, Toru
Sato, Goro
Sato, Yoichi
Sato, Kosuke
Sato, Rie
Sawada, Makoto
Schartel, Norbert
Serlemitsos, Peter
Seta, Hiromi
Shibano, Yasuko
Shida, Maki
Shidatsu, Megumi
Shimada, Takanobu
Shinozaki, Keisuke
Shirron, Peter
Simionescu, Aurora
Simmons, Cynthia
Smith, Randall
Sneiderman, Gary
Soong, Yang
Stawarz, Lukasz
Sugawara, Yasuharu
Sugita, Hiroyuki
Sugita, Satoshi
Szymkowiak, Andrew
Tajima, Hiroyasu
Takahashi, Hiromitsu
Takeda, Shin'ichiro
Takei, Yoh
Tamagawa, Toru
Tamura, Takayuki
Tamura, Keisuke
Tanaka, Takaaki
Tanaka, Yasuo
Tanaka, Yasuyuki
Tashiro, Makoto
Tawara, Yuzuru
Terada, Yukikatsu
Terashima, Yuichi
Tombesi, Francesco
Tomida, Hiroshi
Tsuboi, Yohko
Tsujimoto, Masahiro
Tsunemi, Hiroshi
Tsuru, Takeshi
Uchida, Hiroyuki
Uchiyama, Yasunobu
Uchiyama, Hideki
Ueda, Yoshihiro
Ueda, Shutaro
Ueno, Shiro
Uno, Shin'ichiro
Urry, Meg
Ursino, Eugenio
de Vries, Cor
Wada, Atsushi
Watanabe, Shin
Watanabe, Tomomi
Werner, Norbert
Wik, Daniel
Wilkins, Dan
Williams, Brian
Yamada, Takahiro
Yamada, Shinya
Yamaguchi, Hiroya
Yamaoka, Kazutaka
Yamasaki, Noriko
Yamauchi, Makoto
Yamauchi, Shigeo
Yaqoob, Tahir
Yatsu, Yoichi
Yonetoku, Daisuke
Yoshida, Atsumasa
Yuasa, Takayuki
Zhuravleva, Irina
Zoghbi, Abderahmen
BE DenHerder, JWA
Takahashi, T
Bautz, M
TI The ASTRO-H (Hitomi) X-ray Astronomy Satellite
SO SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Space Telescopes and Instrumentation - Ultraviolet to
Gamma Ray
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE X-ray; Hard X-ray; Gamma-ray; X-ray Astronomy; Gamma-ray Astronomy;
microcalorimeter
ID ONBOARD; SUZAKU; G21.5-0.9; MISSION; NUSTAR
AB The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.
C1 [Takahashi, Tadayuki; Kokubun, Motohide; Mitsuda, Kazuhisa; Baluta, Chris; Bando, Nobutaka; Dotani, Tadayasu; Ebisawa, Ken; Guainazzi, Matteo; Hagino, Kouichi; Harayama, Atsushi; Hayashi, Katsuhiro; Hirose, Kazuyuki; Iizuka, Ryo; Inoue, Yoshiyuki; Inoue, Hajime; Ishida, Manabu; Ishimura, Kosei; Iwata, Naoko; Kawano, Taro; Kawasaki, Shigeo; Koyama, Shu; Lee, Shiu-Hang; Maeda, Yoshitomo; Minesugi, Kenji; Nakagawa, Takao; Nakashima, Shinya; Natsukari, Chikara; Odaka, Hirokazu; Ogawa, Hiroyuki; Ogawa, Mina; Ohta, Masayuki; Okazaki, Tsuyoshi; Ozaki, Masanobu; Sakai, Shin-ichiro; Sameshima, Hiroaki; Sato, Goro; Sato, Rie; Shibano, Yasuko; Shida, Maki; Shimada, Takanobu; Simionescu, Aurora; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Ueno, Shiro; Wada, Atsushi; Watanabe, Shin; Yamada, Takahiro; Yamasaki, Noriko] Japan Aerosp Explorat Agcy JAXA, ISAS, Kanagawa 2525210, Japan.
[Kelley, Richard; Angelini, Lorella; Bialas, Thomas; Boyce, Kevin; Canavan, Edgar; Chiao, Meng; DiPirro, Michael; Eckart, Megan; Hamaguchi, Kenji; Harrus, Ilana; Hornschemeier, Ann; Kallman, Timothy; Kilbourne, Caroline; Kimball, Mark; Krimm, Hans; Leutenegger, Maurice; Markevitch, Maxim; Masters, Candace; Mcguinness, Daniel; Miko, Joseph; Mori, Hideyuki; Moseley, Harvey; Muench, Theodore; Mukai, Koji; Okajima, Takashi; Petre, Robert; Pontius, James; Porter, F. Scott; Pottschmidt, Katja; Sakai, Kazuhiro; Serlemitsos, Peter; Shirron, Peter; Simmons, Cynthia; Sneiderman, Gary; Soong, Yang; Tombesi, Francesco; Watanabe, Tomomi; Williams, Brian; Yamaguchi, Hiroya; Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ohashi, Takaya; Axelsson, Magnus; Ezoe, Yuichiro; Ichinohe, Yuto; Ishisaki, Yoshitaka; Seta, Hiromi; Yamada, Shinya] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan.
[Aharonian, Felix; Chernyakova, Maria] Dublin Inst Adv Studies, Astron & Astrophys Sect, Dublin 2, Ireland.
[Akamatsu, Hiroki; Costantini, Elisa; de Plaa, Jelle; den Herder, Jan-Willem; Giustini, Margherita; Gu, Liyi; Haas, Daniel; Kaastra, Jelle; Mehdipour, Missagh; de Vries, Cor] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Akimoto, Fumie; Furuzawa, Akihiro; Hayashi, Takayuki; Ishibashi, Kazunori; Kunieda, Hideyo; Mitsuishi, Ikuyuki; Miyazawa, Takuya; Nagano, Housei; Tajima, Hiroyasu; Tamura, Keisuke; Tawara, Yuzuru; Yamaoka, Kazutaka] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan.
[Allen, Steve; Asai, Makoto; Blandford, Roger; Gilmore, Kirk; Kamae, Tuneyoshi; King, Ashley; Madejski, Grzegorz; Werner, Norbert; Zhuravleva, Irina] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Anabuki, Naohisa; Hayashida, Kiyoshi; Nagino, Ryo; Nakajima, Hiroshi; Tsunemi, Hiroshi] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Arnaud, Keith; Kara, Erin; Loewenstein, Michael; Mushotzky, Richard; Reynolds, Christopher] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Audard, Marc; Azzarello, Philipp; Ferrigno, Carlo; Paltani, Stephane; Pohl, Martin] Univ Genoa, Dept Astron, CH-1290 Versoix, Switzerland.
[Awaki, Hisamitsu; Ogi, Keiji; Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Bamba, Aya; Nakazawa, Kazuhiro; Ueda, Yoshihiro] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Bautz, Marshall; Bulbul, Esra; Miller, Eric] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Brenneman, Laura; Foster, Adam; Smith, Randall] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Brown, Greg] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Cackett, Edward; Fabian, Andrew; Pinto, Ciro; Russell, Helen] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Coppi, Paolo; Szymkowiak, Andrew; Urry, Meg] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Doty, John] Noqsi Aerosp Ltd, Pine, CO 80470 USA.
[Enoto, Teruaki; Mineshige, Shin] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
[Fujimoto, Ryuichi; Murakami, Toshio; Yonetoku, Daisuke] Kanazawa Univ, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan.
[Fukazawa, Yasushi; Katsuta, Junichiro; Kitaguchi, Takao; Mizuno, Tsunefumi; Ohno, Masanori; Takahashi, Hiromitsu; Tanaka, Yasuyuki] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Galeazzi, Massimiliano; Ursino, Eugenio] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Gallo, Luigi; Wilkins, Dan] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Gandhi, Poshak] Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Goldwurm, Andrea; Laurent, Philippe; Lebrun, Francois; Limousin, Olivier; Maier, Daniel] CEA Saclay, IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Haba, Yoshito] Aichi Univ Educ, Dept Phys & Astron, Kariya, Aichi 4488543, Japan.
[Hatsukade, Isamu; Mori, Koji; Nishioka, Yusuke; Yamauchi, Makoto] Miyazaki Univ, Dept Appl Phys & Elect Engn, Miyazaki 8892192, Japan.
[Hiraga, Junko] Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, Sanda, Hyogo 6691337, Japan.
[Hoshino, Akio; Khangulyan, Dmitry; Kitamoto, Shunji; Saito, Shinya; Uchiyama, Yasunobu] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan.
[Hughes, John] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Wik, Daniel] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ishikawa, Kumi; Tamagawa, Toru; Yuasa, Takayuki] RIKEN Nishina Ctr, Saitama 3510198, Japan.
[Itoh, Masayuki] Kobe Univ, Grad Sch Human Dev & Environm, Kobe, Hyogo 6578501, Japan.
[Iyomoto, Naoko] Kyushu Univ, Fukuoka 8190395, Japan.
[Jewell, Chris; Kretschmar, Peter; Lumb, David; Parmar, Arvind; Schartel, Norbert] ESA, European Space Res & Technol Ctr ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Kataoka, Jun] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan.
[Katsuda, Satoru; Sugawara, Yasuharu; Tsuboi, Yohko] Chuo Univ, Dept Phys, Tokyo 1128551, Japan.
[Kawaharada, Madoka; Okamoto, Atsushi; Sato, Yoichi; Shinozaki, Keisuke; Sugita, Hiroyuki] Japan Aerosp Explorat Agcy JAXA, Tsukuba Space Ctr TKSC, Tsukuba, Ibaraki 3058505, Japan.
[Kawai, Nobuyuki; Sugita, Satoshi; Yatsu, Yoichi] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan.
[Kitayama, Tetsu] Toho Univ, Dept Phys, Chiba 2748510, Japan.
[Kohmura, Takayoshi] Tokyo Univ Sci, Dept Phys, Chiba 2788510, Japan.
[Kosaka, Tatsuro] Kochi Univ Technol, Sch Syst Engn, Kochi 7828502, Japan.
[Koujelev, Alex; Moroso, Franco] Canadian Space Agcy, John H Chapman Space Ctr, Space Explorat Dev Space Explorat, Longueuil, PQ J3Y 8Y9, Canada.
[Koyama, Katsuji; Tanaka, Takaaki; Tsuru, Takeshi; Uchida, Hiroyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
[Kubota, Aya] Shibaura Inst Technol, Dept Elect Informat Syst, Saitama 3378570, Japan.
[Long, Knox] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Makishima, Kazuo; Shidatsu, Megumi] RIKEN, Saitama 3510198, Japan.
[Matsumoto, Hironori] Nagoya Univ, Kobayashi Masukawa Inst, Nagoya, Aichi 4648602, Japan.
[Matsushita, Kyoko; Sasaki, Toru; Sato, Kosuke] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan.
[McCammon, Dan] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[McNamara, Brian] Univ Waterloo, Waterloo, ON N2L 3G1, Canada.
[Miller, Jon; Zoghbi, Abderahmen] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Murakami, Hiroshi] Tohoku Gakuin Univ, Dept Informat Sci, Fac Liberal Arts, Sendai, Miyagi 9813193, Japan.
[Nakamori, Takeshi] Yamagata Univ, Fac Sci, Dept Phys, Yamagata 9908560, Japan.
[Nakano, Toshio] Univ Tokyo, Res Ctr Early Universe, Tokyo 1130033, Japan.
[Namba, Yoshiharu] Chubu Univ, Dept Mech Engn, Kasugai, Aichi 4878501, Japan.
[Nobukawa, Masayoshi] Nara Univ Educ, Dept Teacher Training, Nara 6308528, Japan.
[Nobukawa, Masayoshi] Nara Univ Educ, Sch Educ, Nara 6308528, Japan.
[Noda, Hirofumi] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan.
[Nomachi, Masaharu] Osaka Univ, Nucl Phys Res Ctr, Osaka 5600043, Japan.
[O' Dell, Steve; Ramsey, Brian] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Nobukawa, Kumiko; Ota, Naomi; Yamauchi, Shigeo] Nara Womens Univ, Fac Sci, Dept Phys, Nara 6308506, Japan.
[Paerels, Frits] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
[Sawada, Makoto; Yoshida, Atsumasa] Aoyama Gakuin Univ, Dept Phys & Math, Kanagawa 2525258, Japan.
[Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Takeda, Shin'ichiro] Okinawa Inst Sci & Technol Grad Univ OIST, Adv Med Instrumentat Unit, Okinawa 9040495, Japan.
[Tashiro, Makoto; Terada, Yukikatsu] Saitama Univ, Dept Phys, Saitama 3388570, Japan.
[Uchiyama, Hideki] Shizuoka Univ, Fac Educ, Sci Educ, Shizuoka 4228529, Japan.
[Uno, Shin'ichiro] Nihon Fukushi Univ, Fac Hlth Sci, Handa, Aichi 4750012, Japan.
RP Takahashi, T (reprint author), Japan Aerosp Explorat Agcy JAXA, ISAS, Kanagawa 2525210, Japan.
OI , kouichi/0000-0003-4235-5304
NR 74
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0189-5; 978-1-5106-0190-1
J9 PROC SPIE
PY 2016
VL 9905
AR UNSP 99050U
DI 10.1117/12.2232379
PN 1
PG 17
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WP
UT WOS:000387731500019
ER
PT S
AU Hunt, G
Slater, G
AF Hunt, Gene
Slater, Graham
BE Futuyma, DJ
TI Integrating Paleontological and Phylogenetic Approaches to
Macroevolution
SO ANNUAL REVIEW OF ECOLOGY, EVOLUTION, AND SYSTEMATICS, VOL 47
SE Annual Review of Ecology Evolution and Systematics
LA English
DT Review; Book Chapter
DE diversification; fossil record; molecular phylogeny; phylogenetic
comparative methods; trait evolution
ID BODY-SIZE EVOLUTION; CRETACEOUS-PALEOGENE BOUNDARY;
DIVERGENCE-TIME-ESTIMATION; FOSSIL RECORD; MOLECULAR PHYLOGENIES;
EXTINCTION RATES; COPES RULE; TRAIT EVOLUTION; MORPHOLOGICAL EVOLUTION;
PUNCTUATED EQUILIBRIUM
AB With proliferation of molecular phylogenies and advances in statistical modeling, phylogeneticists can now address macroevolutionary questions that had traditionally been the purview of paleontology. Interest has focused on three areas at the intersection of phylogenetic and paleontological research: time-scaling phylogenies, understanding trait evolution, and modeling species diversification. Fossil calibrations have long been crucial for scaling phylogenies to absolute time, but recent advances allow more equal integration of extinct taxa. Simulation and empirical studies have shown that fossil data can markedly improve inferences about trait evolution, especially for models with heterogeneous temporal dynamics and in clades for which the living forms are unrepresentative remnants of their larger clade. Recent years have also seen a productive cross-disciplinary conversation about the nature and uncertainties of inferring diversification dynamics. Challenges remain, but the present time represents a flowering of interest in integrating these two views on the history of life.
C1 [Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
[Slater, Graham] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
RP Hunt, G (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
EM hunte@si.edu; gslater@uchicago.edu
NR 161
TC 0
Z9 0
U1 13
U2 13
PU ANNUAL REVIEWS
PI PALO ALTO
PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA
SN 1543-592X
BN 978-0-8243-1447-7
J9 ANNU REV ECOL EVOL S
JI Annu. Rev. Ecol. Evol. Syst.
PY 2016
VL 47
BP 189
EP 213
DI 10.1146/annurev-ecolsys-112414-054207
PG 25
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA BG5MY
UT WOS:000389576500009
ER
PT J
AU Hernandez-Kantun, JJ
Gabrielson, P
Hughey, JR
Pezzolesi, L
Rindi, F
Robinson, NM
Pena, V
Riosmena-Rodriguez, R
Le Gall, L
Adey, W
AF Hernandez-Kantun, Jazmin J.
Gabrielson, Paul
Hughey, Jeffery R.
Pezzolesi, Laura
Rindi, Fabio
Robinson, Nestor M.
Pena, Viviana
Riosmena-Rodriguez, Rafael
Le Gall, Line
Adey, Walter
TI Reassessment of branched Lithophyllum spp. (Corallinales, Rhodophyta) in
the Caribbean Sea with global implications
SO PHYCOLOGIA
LA English
DT Article
DE Algal ridges; Lithophyllum congestum; Lithophyllum daedaleum;
Lithophyllum kaiseri; Lithophyllum neocongestum sp nov.; Lithophyllum
platyphyllum; Lithophyllum pseudoplatyphyllum sp nov.; psbA; rbcL;
Sequencing type material; Systematics
ID PHYMATOLITHON-CALCAREUM; GENUS LITHOPHYLLUM; INDIAN-OCEAN; CORAL-REEFS;
SP-NOV; DIVERSITY; ALGAE
AB Plastid-encoded rbcL and psbA sequences from branched, Caribbean Sea Lithophyllum specimens indicate that four species are present, not one. Short (263 base pairs) rbcL sequences from an isolectotype of L. kaiseri (Gulf of Suez) and the holotypes of L. congestum, L. daedaleum and L. platyphyllum (Caribbean Sea) show that L. congestum and L. daedaleum are conspecific with L. kaiseri, the last having nomenclatural priority. Lithophyllum platyphyllum, currently considered a synonym of L. congestum, is recognised as a valid species. Lithophyllum stictaeforme, originally described from the Mediterranean Sea, is not conspecific with L. kaiseri (as L. congestum) as previously suggested. Lithophyllum neocongestum sp. nov. and L. pseudoplatyphyllum sp. nov. are proposed. Together with L. platyphyllum, these three branched species are so far endemic to the Caribbean Sea. This is the first report, documented by DNA sequence data, of a coralline species (L. kaiseri) widespread through the tropical Indo-West Pacific Oceans, Red Sea and Caribbean Sea.
C1 [Hernandez-Kantun, Jazmin J.; Adey, Walter] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20013 USA.
[Gabrielson, Paul] Univ N Carolina, Dept Biol, Coker Hall CB 3280, Chapel Hill, NC 27599 USA.
[Gabrielson, Paul] Univ N Carolina, Herbarium, Coker Hall CB 3280, Chapel Hill, NC 27599 USA.
[Hughey, Jeffery R.] Hartnell Coll, Div Math Sci & Engn, 411 Cent Ave, Salinas, CA 93901 USA.
[Pezzolesi, Laura; Rindi, Fabio] Univ Politecn Marche, Dipartimento Sci Vita & Ambiente, Via Brecce Bianche, I-60131 Ancona, Italy.
[Robinson, Nestor M.; Riosmena-Rodriguez, Rafael] Univ Autonoma Baja California Sur, Dept Biol Marina, Programa Invest Bot Marina, La Paz 23080, Baja Calif Sur, Mexico.
[Pena, Viviana] Univ A Coruna, Fac Ciencias, BIOCOST Res Grp, Dept Biol Anim Biol Vexetal & Ecol, Campus A Coruna, La Coruna 15071, Spain.
[Pena, Viviana] Sorbonne Univ, Museum Natl Hist Nat, UPMC, UMR 7205,CNRS,EPHE,Inst Systemat Evolut Biodivers, 57 Rue Cuvier,CP 39, F-75005 Paris, France.
[Pena, Viviana] Univ Ghent, Phycol Res Grp, Krijgslaan 281,Bldg S8, B-9000 Ghent, Belgium.
[Le Gall, Line] Sorbonne Univ, Museum Natl Hist Nat, UPMC,EPHE, Equipe Explorat Especes & Evolut,UMR 7205,CNRS,In, 57 Rue Cuvier,CP 39, F-75005 Paris, France.
RP Hernandez-Kantun, JJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20013 USA.
EM jaz1083@gmail.com
OI Pena, Viviana/0000-0001-7003-3850; PEZZOLESI, LAURA/0000-0002-6260-2715;
Robinson, Nestor M./0000-0001-7442-1666
FU Smithsonian Institution; National Science Foundation (NSF)
[DEB-0919508]; NSF [DEB-0742437]; Universidade da Coruna; postdoctoral
program Axudas de apoio a etapa inicial de formacion postdoutoral, Plan
I2C (Xunta de Galicia); Total Foundation; Prince Albert II of Monaco
Foundation; Stavros Niarchos Foundation under "Our Planet Reviewed'',
initiative of Museum National d'Histoire Naturelle; Institut
d'Halieutique et des Sciences Marines, University of Toliara; Madagascar
bureau of Wildlife Conservation Society; Stavros Niarchos Foundation
under "Our Planet Reviewed'', initiative of Pro Natura International
FX Foremost, we dedicate this work to our beloved friend and colleague, Dr.
Rafael Riosmena Rodriguez, who suddenly passed away. We thank collectors
Robert Steneck, Will Schmidt, Daniela Gabriel, Thomas Sauvage, Suzanne
Fredericq, Sara Kaleb, Annalisa Falace and Bryan Wysor. The help of
curators at NY and TRH is greatly appreciated for providing fragments or
loans of the type material. J.J. H.-K. thanks the Smithsonian
Institution for a postdoctoral fellowship, a fellowship to attend the
2012 Tropical Field Phycology course at the Smithsonian's Bocas del Toro
Research Station and the help of staff at National Museum of Natural
History Laboratories of Analytical Biology. Collections from Red Sea
localities were supported by National Science Foundation (NSF)
DEB-0919508; some Panama collections were supported by NSF DEB-0742437.
DNA extraction and sequencing performed by J.R.H. were funded by the
generous support from a private family trust (P.W.G.). V.P.F.
acknowledges support by Universidade da Coruna and by the postdoctoral
program Axudas de apoio a etapa inicial de formacion postdoutoral, Plan
I2C (Xunta de Galicia). The specimen PC0165991 was collected during the
Atimo Vatae expedition (principal investigator Philippe Bouchet), funded
by the Total Foundation, Prince Albert II of Monaco Foundation, and
Stavros Niarchos Foundation under "Our Planet Reviewed'', a joint
initiative of Museum National d'Histoire Naturelle and Pro Natura
International in partnership with Institut d'Halieutique et des Sciences
Marines, University of Toliara and the Madagascar bureau of Wildlife
Conservation Society. The Institut de Recherche pour le Developpement
deployed its research catamaran Antea.
NR 43
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U1 1
U2 1
PU INT PHYCOLOGICAL SOC
PI LAWRENCE
PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0031-8884
J9 PHYCOLOGIA
JI Phycologia
PY 2016
VL 55
IS 6
BP 619
EP 639
DI 10.2216/16-7.1
PG 21
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA EF3ZD
UT WOS:000390263000002
ER
PT J
AU Flinte, V
Viana, JH
Macedo, MV
Windsor, D
Sekerka, L
AF Flinte, Vivian
Viana, Jessica Herzog
Macedo, Margarete Valverde
Windsor, Donald
Sekerka, Lukas
TI Revalidation and redescription of three distinct species synonymized as
Plagiometriona sahlbergi (Coleoptera: Chrysomelidae: Cassidinae)
SO ACTA ENTOMOLOGICA MUSEI NATIONALIS PRAGAE
LA English
DT Article
DE Coleoptera; Chrysomelidae; Cassidinae; Plagiometriona; synonymy;
phylogeny; cytochrome oxidase I; morphology; Atlantic Forest; Brazil;
Neotropical Region
ID RIO-DE-JANEIRO; TORTOISE BEETLES; BRAZIL; FOREST
AB Plagiometriona sahlbergi (Boheman, 1855), P. multisignata (Boheman, 1855) and P. scenica (Boheman, 1855) were described over a century and half ago as separate species based on dry museum specimens. The latter two were later synonymized with P. sahlbergi. While observations in nature find both P. sahlbergi and P. multisignata co-occurring on the same host plant, subtle morphological differences suggested they may be distinct species. We tested the validity of the original species separation using additional morphological characters and available molecular sequence data. The new evidence supports Boheman's original separation of species. Accordingly we remove P. multisignata stat. restit. and P. scenica stat. restit. from synonymy with P. sahlbergi and restore their species status. Mitochondrial gene sequence data suggest that P. sahlbergi and P. multisignata bear a closer relationship to other sympatric Plagiometriona species than they do to one another, raising the possibility that these two species have convergent morphologies due to their shared food plant. Biological and ecological notes are also given for these two sympatric species.
C1 [Flinte, Vivian; Viana, Jessica Herzog; Macedo, Margarete Valverde] Univ Fed Rio de Janeiro, Dept Ecol IB, Lab Ecol Insetos, CP 68020, BR-21941590 Rio De Janeiro, RJ, Brazil.
[Viana, Jessica Herzog] Museu Paraense Emilio Goeldi, Coordenacao Zool, Campus Pesquisas, BR-66077830 Belem, Para, Brazil.
[Windsor, Donald] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
[Sekerka, Lukas] Natl Museum, Dept Entomol, Cirkusova 1740, CZ-19300 Prague, Czech Republic.
RP Flinte, V (reprint author), Univ Fed Rio de Janeiro, Dept Ecol IB, Lab Ecol Insetos, CP 68020, BR-21941590 Rio De Janeiro, RJ, Brazil.
EM flinte@biologia.ufrj.br; biojessica@gmail.com; windsord@si.edu;
sagrinae@gmail.com
FU PDJ/CNPq scholarship; INCT HYMPAR Sudeste Brasil (CNPq); INCT HYMPAR
Sudeste Brasil (CAPES); INCT HYMPAR Sudeste Brasil (FAPESP); PENSA-Rio
(FAPERJ); PVE [CNPq400261/2014-6]; Ministry of Culture of the Czech
Republic [DKRVO 2016/14]; Ministry of Culture of the Czech Republic
(National Museum) [00023272]
FX We are grateful to Sama de Freitas for species rearing and C.
Cronemberger from ICMBIO/PARNASO for logistic support (research
authorizations 214/2005, 246/2006 and 13424-1). We also thank Dr. Todd
Barkman (Western Michigan University) for host plant sequencing. VF
received a PDJ/CNPq scholarship. The authors thank INCT HYMPAR Sudeste
Brasil (via CNPq, CAPES and FAPESP), PENSA-Rio (FAPERJ) and PVE (via
CNPq400261/2014-6) for financial support, and the STRI (Smithsonian
Tropical Research Institute, Panama) for logistical support. LS is
grateful to Johannes Bergsten (Naturhistoriska Riksmuseet, Stockholm)
and Johannes Frisch (Museum fur Naturkunde, Berlin) for support during
museum visits and access to type specimens used in this study. This work
was partly financed by the Ministry of Culture of the Czech Republic
(DKRVO 2016/14, National Museum, 00023272).
NR 14
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U1 0
U2 0
PU NARODNI MUZEUM - PRIRODOVEDECKE MUZEUM
PI PRAHA
PA KUNRATICE, PRAHA, CZ-148 00, CZECH REPUBLIC
SN 0374-1036
EI 1804-6487
J9 ACTA ENT MUS NAT PRA
JI Acta Entomol. Mus. Natl. Pragae
PY 2016
VL 56
IS 2
BP 743
EP 754
PG 12
WC Entomology
SC Entomology
GA EE7BE
UT WOS:000389768300015
ER
PT S
AU Gilbert, GS
Parker, IM
AF Gilbert, Gregory S.
Parker, Ingrid M.
BE Leach, JE
Lindow, S
TI The Evolutionary Ecology of Plant Disease: A Phylogenetic Perspective
SO ANNUAL REVIEW OF PHYTOPATHOLOGY, VOL 54
SE Annual Review of Phytopathology
LA English
DT Review; Book Chapter
DE phylogenetic signal; host range; phylogenetic ecology; disease in
natural ecosystems; pathogen spillover; dilution effect; nonhost
resistance; community disease dynamics
ID EMERGING INFECTIOUS-DISEASES; PATHOGEN SPECIES RICHNESS; NBS-LRR
PROTEINS; NATURAL ENEMIES; RAIN-FOREST; SEEDLING MORTALITY; FUNGAL
PATHOGENS; TROPICAL FOREST; SOIL FEEDBACK; HOST PLANTS
AB An explicit phylogenetic perspective provides useful tools for phytopathology and plant disease ecology because the traits of both plants and microbes are shaped by their evolutionary histories. We present brief primers on phylogenetic signal and the analytical tools of phylogenetic ecology. We review the literature and find abundant evidence of phylogenetic signal in pathogens and plants for most traits involved in disease interactions. Plant nonhost resistance mechanisms and pathogen housekeeping functions are conserved at deeper phylogenetic levels, whereas molecular traits associated with rapid coevolutionary dynamics are more labile at branch tips. Horizontal gene transfer disrupts the phylogenetic signal for some microbial traits. Emergent traits, such as host range and disease severity, show clear phylogenetic signals. Therefore pathogen spread and disease impact are influenced by the phylogenetic structure of host assemblages. Phylogenetically rare species escape disease pressure. Phylogenetic tools could be used to develop predictive tools for phytosanitary risk analysis and reduce disease pressure in multispecies cropping systems.
C1 [Gilbert, Gregory S.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA.
[Parker, Ingrid M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA.
[Gilbert, Gregory S.; Parker, Ingrid M.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA.; Gilbert, GS (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
EM ggilbert@ucsc.edu; imparker@ucsc.edu
NR 190
TC 0
Z9 0
U1 9
U2 9
PU ANNUAL REVIEWS
PI PALO ALTO
PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA
SN 0066-4286
BN 978-0-8243-1354-8
J9 ANNU REV PHYTOPATHOL
JI Annu. Rev. Phytopathol.
PY 2016
VL 54
BP 549
EP 578
PG 30
WC Plant Sciences
SC Plant Sciences
GA BG5TJ
UT WOS:000389751400024
PM 27359365
ER
PT S
AU Lehner, MJ
Wang, SY
Reyes-Ruiz, M
Alcock, C
Castro, J
Chen, WP
Chu, YH
Cook, KH
Figueroa, L
Geary, JC
Huang, CK
Kim, DW
Norton, T
Szentgyorgyi, A
Yen, WL
Zhang, ZW
AF Lehner, Matthew J.
Wang, Shiang-Yu
Reyes-Ruiz, Mauricio
Alcock, Charles
Castro, Joel
Chen, Wen-Ping
Chu, You-Hua
Cook, Kem H.
Figueroa, Liliana
Geary, John C.
Huang, Chung-Kai
Kim, Dae-Won
Norton, Timothy
Szentgyorgyi, Andrew
Yen, Wei-Ling
Zhang, Zhi-Wei
BE Hall, HJ
Gilmozzi, R
Marshall, HK
TI Status of the Transneptunian Automated Occultation Survey (TAOS II)
SO GROUND-BASED AND AIRBORNE TELESCOPES VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Telescopes VI
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE TAOS; occultations; San Pedro Martir; high-speed imaging; Transneptunian
Objects; Kuiper Belt Objects; Solar System; telescope array
ID KUIPER-BELT OBJECTS; JUPITER-FAMILY COMETS; TRANS-NEPTUNIAN OBJECTS;
OUTER SOLAR-SYSTEM; SIZE DISTRIBUTION; STELLAR OCCULTATIONS; COLLISIONAL
EVOLUTION; LUMINOSITY FUNCTION; SMALL BODIES; SEARCH
AB The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small (similar to 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (< 10(-3) events per star per year) and short in duration (similar to 200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronomico Nacional at San Pedro Martir in Baja California, Mexico. With a 2.3 square degree held of view and a, high speed camera comprising CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a readout cadence of 20 Hz. Construction of the site began in the fall of 2013, and the survey will begin in the summer of 2017.
C1 [Lehner, Matthew J.; Wang, Shiang-Yu; Chu, You-Hua; Cook, Kem H.; Huang, Chung-Kai; Kim, Dae-Won; Yen, Wei-Ling; Zhang, Zhi-Wei] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19125 USA.
[Lehner, Matthew J.; Alcock, Charles; Geary, John C.; Norton, Timothy; Szentgyorgyi, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Carden St, Cambridge, MA 02138 USA.
[Reyes-Ruiz, Mauricio; Figueroa, Liliana] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada 22800, Baja California, Mexico.
[Chen, Wen-Ping] Natl Cent Univ, Inst Astron, 300 Jhongda Rd, Jhongli 32054, Taiwan.
RP Lehner, MJ (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.; Lehner, MJ (reprint author), Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19125 USA.; Lehner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Carden St, Cambridge, MA 02138 USA.
EM mlehner@asiaa.sinica.edu.tw
NR 53
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0191-8; 978-1-5106-0192-5
J9 PROC SPIE
PY 2016
VL 9906
AR UNSP 99065M
DI 10.1117/12.2232203
PN 1
PG 10
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WM
UT WOS:000387731100171
ER
PT S
AU Matsushita, S
Asaki, Y
Fomalont, EB
Barkats, L
Corder, SA
Hills, RE
Kawabe, R
Maud, LT
Morita, KI
Nikolic, B
Tilanus, RPJ
Vlahakis, C
AF Matsushita, Satoki
Asaki, Yoshiharu
Fomalont, Edward B.
Barkats, Lenis
Corder, Stuartt A.
Hills, Richard E.
Kawabe, Ryohei
Maud, Luke T.
Morita, Koh-Ichiro
Nikolic, Bojan
Tilanus, Remo P. J.
Vlahakis, Catherine
BE Hall, HJ
Gilmozzi, R
Marshall, HK
TI Atmospheric Phase Characteristics of the ALMA Long Baseline
SO GROUND-BASED AND AIRBORNE TELESCOPES VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Telescopes VI
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE ALMA; long baseline; atmospheric phase; fluctuation; phase correction
ID PAIRED ANTENNAS METHOD; PAMPA-LA-BOLA; WATER-VAPOR; COMPENSATION
EXPERIMENTS; CAMPAIGN OBSERVATIONS; COMPLEX PERMITTIVITY; FTS
MEASUREMENTS; 1 THZ; ARRAY; MODEL
AB Atacama Large Millimeter/submillimeter Array (ALMA) is the world's largest millimeter / submillimeter (mm / submm) interferometer. Along with science observations, ALMA has performed several long baseline campaigns in the last 6 years to characterize and optimize its long baseline capabilities. To achieve full long baseline capability of ALMA, it is important to understand the characteristics of atmospheric phase fluctuation at long baselines, since it is believed to be the main cause of mm/submm image degradation. For the first time, we present detailed properties of atmospheric phase fluctuation at mm/submm wavelength from baselines up to 15 km in length. Atmospheric phase fluctuation increases as a function of baseline length with a power-law slope close to 0.6, and many of the data display a shallower slope (0.2 - 0.3) at baseline length greater than about 1 km. Some of the data, on the other hand, show a single slope up to the maximum baseline length of around 15 km. The phase correction method based on water vapor radiometers (WVRs) works well, especially for cases with precipitable water vapor (PWV) greater than 1 mm, typically yielding a 50% decrease or more in the degree of phase fluctuation. However, significant amount of atmospheric phase fluctuation still remains after the WVR phase correction; about 200 micron in rms excess path length (rms phase fluctuation in unit of length) even at PWV less than 1 mm. This result suggests the existence of other non-water-vapor sources of phase fluctuation, and emphasizes the need for additional phase correction methods, such as band-to-band and/or fast switching
C1 [Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Asaki, Yoshiharu; Fomalont, Edward B.; Corder, Stuartt A.; Morita, Koh-Ichiro; Vlahakis, Catherine] Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Chile.
[Asaki, Yoshiharu; Barkats, Lenis; Morita, Koh-Ichiro] Natl Astron Observ Japan, Chile Observ, Alonso de Cordova 3107, Santiago 7630355, Chile.
[Fomalont, Edward B.; Corder, Stuartt A.; Vlahakis, Catherine] Natl Radio Astron Observ, 520 Ldgemont Rd, Charlottesville, VA 22903 USA.
[Barkats, Lenis] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA.
[Hills, Richard E.; Nikolic, Bojan] Univ Cambridge, Cavendish Lab, Astrophys Group, JJ Thomson Ave, Cambridge CB3 0HE, England.
[Kawabe, Ryohei] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Kawabe, Ryohei] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Kawabe, Ryohei] Grad Univ Adv Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Maud, Luke T.; Tilanus, Remo P. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Matsushita, S (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
EM satoki@asiaa.sinica.edu.tw
OI Barkats, Denis/0000-0002-8971-1954; Nikolic, Bojan/0000-0001-7168-2705
NR 35
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0191-8; 978-1-5106-0192-5
J9 PROC SPIE
PY 2016
VL 9906
AR UNSP 99064X
DI 10.1117/12.2231846
PN 1
PG 13
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WM
UT WOS:000387731100147
ER
PT S
AU Raffin, P
Ho, PTP
Asada, K
Blundell, R
Bower, GC
Burgos, R
Chang, CC
Chen, MT
Christensen, R
Chu, YH
Grimes, PK
Han, CC
Huang, CWL
Huang, YD
Hsieh, FC
Inoue, M
Koch, PM
Kubo, D
Leiker, S
Lin, L
Liu, CT
Lo, SH
Martin-Cocher, P
Matsushita, S
Nakamura, M
Meyer-Zhao, Z
Nishioka, H
Norton, T
Nystrom, G
Paine, SN
Patel, NA
Pu, HY
Snow, W
Sridharan, TK
Srinivasan, R
Wang, J
AF Raffin, Philippe
Ho, Paul T. P.
Asada, Keiichi
Blundell, Raymond
Bower, Geoffrey C.
Burgos, Roberto
Chang, Chih-Cheng
Chen, Ming-Tang
Christensen, Robert
Chu, You-Hua
Grimes, Paul K.
Han, C. C.
Huang, Chih-Wei L.
Huang, Yau-De
Hsieh, Fang-Chia
Inoue, Makoto
Koch, Patrick M.
Kubo, Derek
Leiker, Steve
Lin, Lupin
Liu, Ching-Tang
Lo, Shih-Hsiang
Martin-Cocher, Pierre
Matsushita, Satoki
Nakamura, Masanori
Meyer-Zhao, Zheng
Nishioka, Hiroaki
Norton, Tim
Nystrom, George
Paine, Scott N.
Patel, Nimesh A.
Pu, Hung-Yi
Snow, William
Sridharan, T. K.
Srinivasan, Ranjani
Wang, Jackie
BE Hall, HJ
Gilmozzi, R
Marshall, HK
TI The Greenland Telescope: Antenna Retrofit Status and Future Plans
SO GROUND-BASED AND AIRBORNE TELESCOPES VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Telescopes VI
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE Greenland; VLBI; antenna retrofit; antenna assembly
AB Since the ALMA North America Prototype Antenna was awarded to the Smithsonian Astrophysical Observatory (SAO), SAO and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA) are working jointly to relocate the antenna to Greenland. This paper shows the status of the antenna retrofit and the work carried out after the recommissioning and subsequent disassembly of the antenna at the VLA has taken place.
The next coming months will see the start of the antenna reassembly at Thule Air Base. These activities are expected to last until the fall of 2017 when commissioning should take place. In parallel, design, fabrication and testing of the last components are taking place in Taiwan.
C1 [Ho, Paul T. P.; Asada, Keiichi; Chang, Chih-Cheng; Chen, Ming-Tang; Chu, You-Hua; Han, C. C.; Huang, Chih-Wei L.; Huang, Yau-De; Inoue, Makoto; Koch, Patrick M.; Lin, Lupin; Lo, Shih-Hsiang; Martin-Cocher, Pierre; Matsushita, Satoki; Nakamura, Masanori; Meyer-Zhao, Zheng; Nishioka, Hiroaki; Nystrom, George; Pu, Hung-Yi; Wang, Jackie] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Blundell, Raymond; Burgos, Roberto; Grimes, Paul K.; Leiker, Steve; Norton, Tim; Paine, Scott N.; Patel, Nimesh A.; Sridharan, T. K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Raffin, Philippe; Bower, Geoffrey C.; Kubo, Derek; Snow, William; Srinivasan, Ranjani] ASIAA Hilo Off, Univ Pk,645 N AOhoku Pl, Hilo, HI 96720 USA.
[Christensen, Robert; Hsieh, Fang-Chia; Liu, Ching-Tang] Natl Chung Shan Inst Sci & Technol, N-300-5,Lane 277,Xi An St, Taichung 407, Taiwan.
RP Raffin, P (reprint author), ASIAA Hilo Off, Univ Pk,645 N AOhoku Pl, Hilo, HI 96720 USA.
EM raffin@asiaa.sinica.edu.tw
NR 8
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0191-8; 978-1-5106-0192-5
J9 PROC SPIE
PY 2016
VL 9906
AR UNSP 99060U
DI 10.1117/12.2232889
PN 1
PG 8
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WM
UT WOS:000387731100026
ER
PT S
AU Richer, MG
Lee, WH
Gonzalez, J
Jannuzi, BT
Sanchez, B
Ortega, FR
Alcock, C
Alonso, AC
Diaz, MTG
Gutierrez, L
Herrera, J
Hill, D
Norton, TJ
Pedrayes, MH
Perez-Calpena, A
Reyes-Ruiz, M
Guerrero, HS
Sierra, G
Teran, J
Urdaibay, D
Uribe, JA
Watson, AM
Zaritsky, D
Vargas, MG
AF Richer, Michael G.
Lee, William H.
Gonzalez, Jesus
Jannuzi, Buell T.
Sanchez, Beatriz
Rosales Ortega, Fabian
Alcock, Charles
Carraminana Alonso, Alberto
Teresa Garcia Diaz, Ma.
Gutierrez, Leonel
Herrera, Joel
Hill, Derek
Norton, Timothy J.
Pedrayes, Maria H.
Perez-Calpena, Ana
Reyes-Ruiz, Mauricio
Serrano Guerrero, Hazael
Sierra, Gerardo
Teran, Jose
Urdaibay, David
Uribe, Jorge A.
Watson, Alan M.
Zaritsky, Dennis
Garcia Vargas, Marisa
BE Hall, HJ
Gilmozzi, R
Marshall, HK
TI The Telescopio San Pedro Martir project
SO GROUND-BASED AND AIRBORNE TELESCOPES VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Telescopes VI
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE TSPM; OAN-SPM; telescope project; optics; enclosure; site; Mexico
ID MAGELLAN; MMT
AB The Telescopio San Pedro Martir project intends to construct a 6.5m telescope to be installed at the Observatorio Astronomico Nacional in the Sierra San Pedro Martir in northern Baja California, Mexico. The project is an association of Mexican institutions, lead by the Instituto Nacional de Astrofisica, Optica y Electronica and the Instituto de Astronomia at the Universidad Nacional Autonoma de Mexico, in partnership with the Smithsonian Astrophysical Observatory and the University of Arizona's Department of Astronomy and Steward Observatory. The project is currently in the planning and design stage. Once completed, the partners plan to operate the MMT and TSPM as a binational astrophysical observatory.
C1 [Richer, Michael G.; Teresa Garcia Diaz, Ma.; Gutierrez, Leonel; Herrera, Joel; Pedrayes, Maria H.; Reyes-Ruiz, Mauricio; Serrano Guerrero, Hazael; Sierra, Gerardo] Univ Nacl Autonoma Mexico, Inst Astron, Km 107 Carr Ensenada Tijuana, Ensenada, BC, Mexico.
[Lee, William H.; Gonzalez, Jesus; Sanchez, Beatriz; Urdaibay, David; Watson, Alan M.] Univ Nacl Autonoma Mexico, Inst Astron, Ciudad Univ, Mexico City, DF, Mexico.
[Jannuzi, Buell T.; Zaritsky, Dennis] Univ Arizona, Dept Astron, 933 North Cherry Ave,Rm N204, Tucson, AZ USA.
[Rosales Ortega, Fabian; Carraminana Alonso, Alberto] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla, Mexico.
[Alcock, Charles; Norton, Timothy J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Hill, Derek; Teran, Jose] M3 Engn & Technol Corp, 2051 W Sunset Rd,Suite 101, Tucson, AZ USA.
[Perez-Calpena, Ana; Garcia Vargas, Marisa] FRACTAL SLNE, C Tulipan 2,P13-1A, E-28231 Madrid, Spain.
[Uribe, Jorge A.] Ctr Ingn & Desarrollo Ind, Av Playa Pie de la Cuesta 702, Queretaro, Queretaro, Mexico.
RP Richer, MG (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Km 107 Carr Ensenada Tijuana, Ensenada, BC, Mexico.
EM richer@astro.unam.mx; wlee@astro.unam.mx
RI Gonzalez, Jose/L-6687-2014
OI Gonzalez, Jose/0000-0002-3724-1583
NR 25
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0191-8; 978-1-5106-0192-5
J9 PROC SPIE
PY 2016
VL 9906
AR UNSP 99065S
DI 10.1117/12.2232000
PN 1
PG 13
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WM
UT WOS:000387731100175
ER
PT S
AU Villanueva, S
Eastman, JD
Gaudi, BS
Pogge, RW
Stassun, KG
Trueblood, M
Trueblood, P
AF Villanueva, S., Jr.
Eastman, J. D.
Gaudi, B. S.
Pogge, R. W.
Stassun, K. G.
Trueblood, M.
Trueblood, P.
BE Hall, HJ
Gilmozzi, R
Marshall, HK
TI DEdicated MONitor of EXotransits and Transients (DEMONEXT): a Low-Cost
Robotic and Automated Telescope for Followup of Exoplanetary Transits
and Other Transient Events
SO GROUND-BASED AND AIRBORNE TELESCOPES VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Ground-Based and Airborne Telescopes VI
CY JUN 26-JUL 01, 2016
CL Edinburgh, SCOTLAND
SP SPIE
DE robotic telescopes; automated telescopes; small telescopes; followup
observations; exoplanets; transits; supernovae
ID HOT JUPITER
AB We present the design and development of the DEdicated MONitor of EXotransits and Transients (DEMONEXT), an automated and robotic 20 inch telescope jointly funded by The Ohio State University and Vanderbilt University. The telescope is a PlaneWave CDK20 f/6.8 Corrected Dall-Kirkham Astrograph telescope on a Mathis Instruments MI-750/1000 Fork Mount located at Winer Observatory in Sonoita, AZ. DEMONEXT has a Hedrick electronic focuser, Finger Lakes Instrumentation (FLI) CFW-3-10 filter wheel, and a 2048 x 2048 pixel FLI Proline CCD3041 camera with a pixel scale of 0.90 arc-seconds per pixel and a 30.7 x 30.7 arc-minute field-of-view. The telescope's automation, controls, and scheduling are implemented in Python, including a facility to add new targets in real time for rapid follow-up of time-critical targets. DEMONEXT will be used for the confirmation and detailed investigation of newly discovered planet candidates from the Kilodegree Extremely Little Telescope (KELT) survey, exploration of the atmospheres of Hot Jupiters via transmission spectroscopy and thermal emission measurements, and monitoring of select eclipsing binary star systems as benchmarks for models of stellar evolution. DEMONEXT will enable rapid confirmation imaging of supernovae, flare stars, tidal disruption events, and other transients discovered by the All Sky Automated Survey for SuperNovae (ASAS-SN). DEMONEXT will also provide follow-up observations of single-transit planets identified by the Transiting Exoplanet Survey Satellite (TESS) mission, and to validate long-period eclipsing systems discovered by Gaia.
C1 [Villanueva, S., Jr.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Eastman, J. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA.
[Trueblood, M.; Trueblood, P.] Winer Observ, POB 797, Sonoita, AZ 85637 USA.
RP Villanueva, S (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
EM svillan@astronomy.ohio-state.edu
NR 18
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-1-5106-0191-8; 978-1-5106-0192-5
J9 PROC SPIE
PY 2016
VL 9906
AR UNSP 99062L
DI 10.1117/12.2231122
PN 1
PG 12
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BG2WM
UT WOS:000387731100075
ER
PT J
AU Montoya-Maya, PH
Smit, KP
Burt, AJ
Frias-Torres, S
AF Montoya-Maya, Phanor H.
Smit, Kaylee P.
Burt, April J.
Frias-Torres, Sarah
TI Large-scale coral reef restoration could assist natural recovery in
Seychelles, Indian Ocean
SO NATURE CONSERVATION-BULGARIA
LA English
DT Article
DE Reef recovery; coral transplantation; coral settlement; coral
recruitment; Acroporidae; Pocilloporidae; Western Indian Ocean
ID ECOLOGICAL RESTORATION; SELF-RECRUITMENT; CLIMATE-CHANGE; DISPERSAL;
FISHES; IDENTIFICATION; RESILIENCE; ECOSYSTEMS; MORTALITY; EVOLUTION
AB The aim of ecological restoration is to establish self-sustaining and resilient systems. In coral reef restoration, transplantation of nursery-grown corals is seen as a potential method to mitigate reef degradation and enhance recovery. The transplanted reef should be capable of recruiting new juvenile corals to ensure long-term resilience. Here, we quantified how coral transplantation influenced natural coral recruitment at a large-scale coral reef restoration site in Seychelles, Indian Ocean. Between November 2011 and June 2014 a total of 24,431 nursery-grown coral colonies from 10 different coral species were transplanted in 5,225 m(2) (0.52 ha) of degraded reef at the no-take marine reserve of Cousin Island Special Reserve in an attempt to assist in natural reef recovery. We present the results of research and monitoring conducted before and after coral transplantation to evaluate the positive effect that the project had on coral recruitment and reef recovery at the restored site. We quantified the density of coral recruits (spat <1 cm) and juveniles (colonies 1-5 cm) at the transplanted site, a degraded control site and a healthy control site at the marine reserve. We used ceramic tiles to estimate coral settlement and visual surveys with 1 m2 quadrats to estimate coral recruitment. Six months after tile deployment, total spat density at the transplanted site (123.4 +/- 13.3 spat m(-2)) was 1.8 times higher than at healthy site (68.4 +/- 7.8 spat m(-2)) and 1.6 times higher than at degraded site (78.2 +/- 7.17 spat m(-2)). Two years after first transplantation, the total recruit density was highest at healthy site (4.8 +/- 0.4 recruits m(-2)), intermediate at transplanted site (2.7 +/- 0.4 recruits m(-2)), and lowest at degraded site (1.7 +/- 0.3 recruits m(-2)). The results suggest that large-scale coral restoration may have a positive influence on coral recruitment and juveniles. The effect of key project techniques on the results are discussed. This study supports the application of large-scale, science-based coral reef restoration projects with at least a 3-year time scale to assist the recovery of damaged reefs.
C1 [Montoya-Maya, Phanor H.; Smit, Kaylee P.; Burt, April J.; Frias-Torres, Sarah] Nat Seychelles, Mahe, Seychelles.
[Smit, Kaylee P.] Nelson Mandela Metropolitan Univ, Dept Oceanog, Port Elizabeth, South Africa.
[Burt, April J.] Seychelles Isl Fdn, Mahe, Seychelles.
[Frias-Torres, Sarah] Smithsonian Marine Stn, Ft Pierce, FL USA.
RP Montoya-Maya, PH (reprint author), Nat Seychelles, Mahe, Seychelles.
EM phanor@phmontoyamaya.com
FU United States Agency for International Development (USAID) Reef Rescuers
Project [674-A-00-10-00123-00]
FX We thank S. Beach, S.C. Klaus, E. Martin, C. Reveret, K. Rowe and N.
Taylor for help during fieldwork. N. Shah and K. Henri at Nature
Seychelles for managing the Reef Rescuers Project. A. Hennie from Black
Pearl Seychelles, for allowing us to use their stereomicroscope. Several
anonymous reviewers gave constructive criticisms improving the
manuscript. Funding to Nature Seychelles was received through the United
States Agency for International Development (USAID) Reef Rescuers
Project 674-A-00-10-00123-00.
NR 53
TC 0
Z9 0
U1 5
U2 5
PU PENSOFT PUBL
PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1314-6947
EI 1314-3301
J9 NAT CONSERV-BULGARIA
JI Nat. Conserv.-Bulgaria
PY 2016
IS 16
BP 1
EP 17
DI 10.3897/natureconservation.16.8604
PG 17
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EE5NJ
UT WOS:000389654600001
ER
PT J
AU Bilby, K
AF Bilby, Kenneth
TI Creole Music of the French West Indies: A Discography 1900-1959
SO NWIG-NEW WEST INDIAN GUIDE-NIEUWE WEST-INDISCHE GIDS
LA English
DT Book Review
C1 [Bilby, Kenneth] Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA.
RP Bilby, K (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA.
EM kmbilby@gmail.com
NR 3
TC 0
Z9 0
U1 0
U2 0
PU KITLV PRESS
PI LEIDEN
PA PO BOX 9515, 2300 RA LEIDEN, NETHERLANDS
SN 1382-2373
J9 NWIG-NEW W INDIAN GU
JI NWIG- New West Indian Guid.
PY 2016
VL 90
IS 3-4
BP 384
EP 386
DI 10.1163/22134360-09003047
PG 3
WC Area Studies; Humanities, Multidisciplinary
SC Area Studies; Arts & Humanities - Other Topics
GA EE6WG
UT WOS:000389753700049
ER
PT J
AU Jaafar, Z
Polgar, G
Zamroni, Y
AF Jaafar, Zeehan
Polgar, Gianluca
Zamroni, Yuliadi
TI Description of a new species of Periophthalmus (Teleostei: Gobiidae)
from the Lesser Sunda Islands
SO RAFFLES BULLETIN OF ZOOLOGY
LA English
DT Article
DE Oxudercinae; mudskipper; cryptic species; ichthyofauna; Sumba Island
ID MUDSKIPPER; OXUDERCINAE; GENUS; KEY
AB We describe Periophthalmus pusing sp. nov., a mudskipper species from the Lesser Sunda Islands. This species closely resembles, and was previously identified as, its congener Periophthalmus gracilis Eggert, 1935. A black spot on the posterior portion of the first dorsal fin, a diagnostic character for P. gracilis, is also present in the new species, and thus led to the earlier confusion. Adults of Periophthalmus pusing sp. nov. (> 30 mm SL) differ from those of Periophthalmus gracilis in having XI-XV spines in the first dorsal-fin (vs. VI-XII in P. gracilis), first dorsal fin taller than depth of body at anus (first dorsal fin shorter than depth of body at anus in Periophthalmus gracilis), interdorsal distance less than half the length of the first dorsal-fin spine (interdorsal distance more than half the length of the first dorsal-fin spine in Periophthalmus gracilis).
C1 [Jaafar, Zeehan] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, POB 37012,MRC 159, Washington, DC 20013 USA.
[Jaafar, Zeehan] Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore.
[Polgar, Gianluca] Univ Brunei Darussalam, Environm & Life Sci Programme, Fac Sci, Jalan Tungku Link,BE 1410, Gadong, Brunei.
[Zamroni, Yuliadi] Mataram Univ, Fac Math & Nat Sci, Biol Study Programme, Jalan Majapahit 62, Mataram 83125, Indonesia.
RP Jaafar, Z (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, POB 37012,MRC 159, Washington, DC 20013 USA.; Jaafar, Z (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore.
EM jaafarz@si.edu
FU Leonard P. Schultz Fund, Smithsonian Institution
FX We thank the following collection managers and curators for facilitating
our examination of fishes under their care: Amanda Hay (AMS), Mark
McGrouther (AMS), Renny Hadiaty (MZB), Jeffrey Clayton (USNM), Kelvin
Lim (ZRC), Tan Heok Hui (ZRC), and Ronald de Ruiter (RMNH). Sandra
Raredon photographed and prepared Fig. 1. Tran Dac Dinh, photographed,
and permitted the use of Fig. 3. The manuscript benefited from the
suggestions made by Edward Murdy and Tan Heok Hui. Specimen collections
complied with ethical guidelines and all stipulations within RISTEK
Permit 421/SIP/FRP/SM/XI/2012 to the first author. Fieldwork and related
expenses were supported by the Leonard P. Schultz Fund, Smithsonian
Institution, awarded to the first author.
NR 9
TC 0
Z9 0
U1 2
U2 2
PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES
PI SINGAPORE
PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE
SN 0217-2445
J9 RAFFLES B ZOOL
JI Raffles Bull. Zool.
PY 2016
VL 64
BP 278
EP 283
PG 6
WC Zoology
SC Zoology
GA EE6JV
UT WOS:000389717300025
ER
PT S
AU Elliott, J
de Souza, RS
Krone-Martins, A
Cameron, E
Ishida, EEO
Hilbe, J
AF Elliott, J.
de Souza, R. S.
Krone-Martins, A.
Cameron, E.
Ishida, E. E. O.
Hilbe, J.
BE Napolitano, NR
Longo, G
Marconi, M
Paolillo, M
Iodice, E
TI Using Gamma Regression for Photometric Redshifts of Survey Galaxies
SO UNIVERSE OF DIGITAL SKY SURVEYS: A MEETING TO HONOUR THE 70TH BIRTHDAY
OF MASSIMO CAPACCIOLI
SE Astrophysics and Space Science Proceedings
LA English
DT Proceedings Paper
CT Meeting on Universe of Digital Sky Surveys
CY NOV 25-28, 2014
CL Naples, ITALY
ID GENERALIZED LINEAR-MODELS
AB Machine learning techniques offer a plethora of opportunities in tackling big data within the astronomical community. We present the set of Generalized Linear Models as a fast alternative for determining photometric redshifts of galaxies, a set of tools not commonly applied within astronomy, despite being widely used in other professions. With this technique, we achieve catastrophic outlier rates of the order of similar to 1%, that can be achieved in a matter of seconds on large datasets of size similar to 1; 000;000. To make these techniques easily accessible to the astronomical community, we developed a set of libraries and tools that are publicly available.
C1 [Elliott, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Elliott, J.] Max Planck Inst Extraterr Phys, Giessenbachstrabe 1, D-85748 Garching, Germany.
[de Souza, R. S.] MTA Eotvos Univ, EIRSA Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Krone-Martins, A.] Univ Lisbon, Fac Ciencias, SIM, Ed C8,Campo Grande, P-1749016 Lisbon, Portugal.
[Cameron, E.] Univ Oxford, Dept Zool, Tinbergen Bldg,South Parks Rd, Oxford OX1 3PS, England.
[Ishida, E. E. O.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
[Hilbe, J.] Arizona State Univ, Tempe, AZ 85287 USA.
[Hilbe, J.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Elliott, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jonathan.elliott@cfa.harvard.edu; rafael.2706@gmail.com;
algol@sim.ul.pt; dr.ewan.cameron@gmail.com; emille@mpa-garching.mpg.de;
j.m.hilbe@gmail.com
OI Krone-Martins, Alberto/0000-0002-2308-6623
NR 14
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 1570-6591
BN 978-3-319-19330-4; 978-3-319-19329-8
J9 ASTROPHYSICS SPACE
PY 2016
VL 42
BP 91
EP 96
DI 10.1007/978-3-319-19330-4_13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BG5XG
UT WOS:000389802600014
ER
PT J
AU Baldwin, CC
Robertson, DR
Nonaka, A
Tornabene, L
AF Baldwin, Carole C.
Robertson, D. Ross
Nonaka, Ai
Tornabene, Luke
TI Two new deep-reef basslets (Teleostei, Grammatidae, Lipogramma), with
comments on the eco-evolutionary relationships of the genus
SO ZOOKEYS
LA English
DT Article
DE Manned submersible; cryptic species; integrative taxonomy; phylogeny;
ocean exploration; Smithsonian Deep Reef Observation Project (DROP)
ID SPECIES DELIMITATION; PHYLOGENETIC ANALYSIS; DISTRIBUTIONAL NOTES; GOBY
TELEOSTEI; MULTIPLE LOCI; SEQUENCE DATA; DNA BARCODES; FISHES;
PERCIFORMES; ANABANTOIDES
AB The banded basslet, Lipogramma evides Robins & Colin, 1979, is shown to comprise two species: L. evides, which inhabits depths of 133-302 m, and a new species described here as Lipogramma levinsoni, which inhabits depths of 108-154 m and previously was considered to represent the juvenile of L. evides. A second new species of banded basslet, described here as Lipogramma haberi, inhabits depths of 152-233 m and was previously not reported in the literature. Morphologically, the three species differ in color patterns and modal numbers of gill rakers, whereas various other morphological features distinguish L. levinsonsi from L. evides and L. haberi. DNA barcode data and multilocus, coalescent-based, species-delimitation analysis support the recognition of the three species. Phylogenetic analysis of mitochondrial and nuclear genetic data supports a sister-group relationship between the two deepest-living of the three species, L. evides and L. haberi, and suggests that the shallower L. levinsoni is more closely related to L. anabantoides Bohlke 1960, which inhabits depths < 120 m. Evolutionary relationships within Lipogramma thus appear to be correlated with species depth ranges, an eco-evolutionary pattern that has been observed in other Caribbean marine teleosts and that warrants further investigation. The new species represent the eleventh and twelfth new fish species described in recent years from exploratory submersible diving in the Caribbean in the globally poorly studied depth zone of 50-300 m. This study suggests that there are at least two additional cryptic species of Lipogramma, which are being analyzed in ongoing investigations of Caribbean deep-reef ecosystems.
C1 [Baldwin, Carole C.; Nonaka, Ai; Tornabene, Luke] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Robertson, D. Ross] Smithsonian Trop Res Inst, Balboa, Panama.
RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
EM baldwinc@si.edu
FU Consortium for Understanding and Sustaining a Biodiverse Planet;
Competitive Grants for the Promotion of Science program; Herbert R. and
Evelyn Axelrod Endowment Fund for systematic ichthyology; STRI funds;
National Geographic Society's Committee for Research and Exploration
[9102-12]
FX We thank Laura Albini, Bruce Brandt, Barry Brown, Mary Brown, Cristina
Castillo, Loretta Cooper, Tico Christiaan, Tommy Devine, Grant Gilmore,
Brian Horne, Brian Huber, Dave Johnson, Rob Loendersloot, Caleb McMahon,
Dan Mulcahy, Jon Norenberg, Diane Pitassy, Sandra Raredon, Rob Robins,
Laureen Schenk, Adriane "Dutch" Schrier, Ian Silver-Gorges, Ashleigh
Smythe and Barbara van Bebber for assistance in various ways with this
study. Funding for the Smithsonian Institution's Deep Reef Observation
Project was provided internally by the Consortium for Understanding and
Sustaining a Biodiverse Planet to CCB, the Competitive Grants for the
Promotion of Science program to CCB and DRR, the Herbert R. and Evelyn
Axelrod Endowment Fund for systematic ichthyology to CCB, and STRI funds
to DRR. Externally the research was funded by National Geographic
Society's Committee for Research and Exploration to CCB (Grant
#9102-12). This is Ocean Heritage Foundation/Curacao Sea
Aquarium/Substation Curacao (OHF/SCA/SC) contribution number 27.
NR 47
TC 1
Z9 1
U1 0
U2 0
PU PENSOFT PUBL
PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1313-2989
EI 1313-2970
J9 ZOOKEYS
JI ZooKeys
PY 2016
IS 638
BP 45
EP 82
DI 10.3897/zookeys.638.10455
PG 38
WC Zoology
SC Zoology
GA EE8QS
UT WOS:000389891400004
PM 28174497
ER
PT J
AU Robertson, DR
Perez-Espana, H
Lara, EN
Itza, FP
Simoes, N
AF Ross Robertson, D.
Perez-Espana, Horacio
Nunez Lara, Enrique
Puc Itza, Francisco
Simoes, Nuno
TI The fishes of Cayo Arcas (Campeche Bank, Gulf of Mexico): an updated
checklist
SO ZOOKEYS
LA English
DT Article
DE Endemic species; invasive damselfish species; reef-fishes; reef-habitat;
southwest Gulf of Mexico
ID KYPHOSIDAE TELEOSTEI PERCIFORMES; CORAL-REEFS; MYLIOBATIFORMES;
MANGROVES; RESOURCE
AB Cayo Arcas is a small, offshore reef complex on the southwest corner of Campeche Bank, Gulf of Mexico. The only published information (from 2000) on the fishes of that reef refers to 37 species. Here additional information is added, some from unpublished observations during the 1980s, as well as author observations made during 2013 and 2016. These bring the checklist of that reef's fishes up to 162 species. The possible effects of the limited number of fish habitats available at Cayo Arcas on the composition of its fish fauna are discussed. The Indo-Pacific damselfish Neopomacentrus cyanomos (Bleeker, 1856) was first recorded in the Atlantic in mid-2013, on shoreline reefs in the southwest corner of the Gulf of Mexico. Recently reviewed underwater photographs show that N. cyanomos also was present at Cayo Arcas in mid2013, 350 km from the first-record site. Hence it evidently had a substantial population in the southwest Gulf of Mexico in 2013, and must have arrived in there long before that year.
C1 [Ross Robertson, D.] Smithsonian Trop Res Inst, Balboa, Panama.
[Perez-Espana, Horacio] Univ Veracruzana, Inst Ciencias Marinas & Pesquerias, Hidalgo 617, Boca Del Rio 94290, Veracruz, Mexico.
[Nunez Lara, Enrique] Univ Autonoma Carmen, Fac Ciencias Nat, Ciudad Del Carmen, Campeche, Mexico.
[Puc Itza, Francisco] CINVESTAV, Unidad Merida, Merida, Yucatan, Venezuela.
[Simoes, Nuno] UNAM, Fac Ciencias, Unidad Multidisciplinaria Docencia & Invest Sisal, Merida, Yucatan, Venezuela.
RP Robertson, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
EM drr@stri.org
FU Harte Institute (Biodiversity of the southern Gulf of Mexico); CONABIO
[NE018]; SEP-CONACyt [69747, 108083]
FX Thanks to Quetzalli Hernandez, whose leadership of the Cayo Arcas
expedition of August 2016 greatly facilitated work there, and to
essential support by the captain (Hector Agustin Torres Murillo) and
crew of the Buque de Investigacion Oceanografico Arm "Hondo" (BI-06),
Secretaria de Marina, Estados Unidos Mexicanos. The 2016 expedition was
financed by grants to NS from the Harte Institute (Biodiversity of the
southern Gulf of Mexico) and CONABIO (NE018; Actualizacion del
conocimiento de la diversidad de especies de invertebrados marinos
bentonicos de aguas someras (< 50m) del Sur del Golfo de Mexico.
Fieldwork in 2013 was funded by SEP-CONACyt grants 69747 to HP-E and
108083 to ENL.
NR 32
TC 0
Z9 0
U1 4
U2 4
PU PENSOFT PUBL
PI SOFIA
PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA
SN 1313-2989
EI 1313-2970
J9 ZOOKEYS
JI ZooKeys
PY 2016
IS 640
BP 139
EP 155
DI 10.3897/zookeys.640.10862
PG 17
WC Zoology
SC Zoology
GA EE8RI
UT WOS:000389893000009
PM 28138290
ER
PT B
AU Blau, S
Ubelaker, DH
AF Blau, Soren
Ubelaker, Douglas H.
BE Blau, S
Ubelaker, DH
TI Forensic Anthropology and Archaeology Moving Forward
SO HANDBOOK OF FORENSIC ANTHROPOLOGY AND ARCHAEOLOGY, 2ND EDITION
SE World Archaeological Congress Research Handbooks in Archaeology
LA English
DT Article; Book Chapter
ID AUSTRALIAN POPULATION; SEXUAL-DIMORPHISM; STATURE; EUROPE
C1 [Blau, Soren] Victorian Inst Forens Med, Southbank, Vic, Australia.
[Blau, Soren] Monash Univ, Dept Forens Med, Clayton, Vic 3800, Australia.
[Blau, Soren] Royal Coll Pathologists Australasia, Fac Sci, Surry Hills, NSW, Australia.
[Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Ubelaker, Douglas H.] George Washington Univ, Washington, DC 20052 USA.
[Ubelaker, Douglas H.] Michigan State Univ, E Lansing, MI 48824 USA.
[Ubelaker, Douglas H.] Amer Acad Forens Sci, Colorado Springs, CO USA.
RP Blau, S (reprint author), Victorian Inst Forens Med, Southbank, Vic, Australia.; Blau, S (reprint author), Monash Univ, Dept Forens Med, Clayton, Vic 3800, Australia.; Blau, S (reprint author), Royal Coll Pathologists Australasia, Fac Sci, Surry Hills, NSW, Australia.
NR 71
TC 0
Z9 0
U1 1
U2 1
PU ROUTLEDGE
PI ABINGDON
PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND
BN 978-1-62958-385-3; 978-1-315-52893-9; 978-1-62958-384-6
J9 WAC RES H ARCHAEOL
PY 2016
BP 1
EP 9
PG 9
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA BG4IX
UT WOS:000388884300002
ER
PT B
AU Ubelaker, DH
AF Ubelaker, Douglas H.
BE Blau, S
Ubelaker, DH
TI Historical Development of Forensic Anthropology Perspectives from the
United States
SO HANDBOOK OF FORENSIC ANTHROPOLOGY AND ARCHAEOLOGY, 2ND EDITION
SE World Archaeological Congress Research Handbooks in Archaeology
LA English
DT Article; Book Chapter
ID AGE-CHANGES; SKELETON; IDENTIFICATION; STATURE; BONES; RACE; SEX; I.
C1 [Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Ubelaker, Douglas H.] George Washington Univ, Washington, DC 20052 USA.
[Ubelaker, Douglas H.] Michigan State Univ, E Lansing, MI 48824 USA.
[Ubelaker, Douglas H.] Amer Acad Forens Sci, Colorado Springs, CO 80904 USA.
RP Ubelaker, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.; Ubelaker, DH (reprint author), George Washington Univ, Washington, DC 20052 USA.; Ubelaker, DH (reprint author), Michigan State Univ, E Lansing, MI 48824 USA.; Ubelaker, DH (reprint author), Amer Acad Forens Sci, Colorado Springs, CO 80904 USA.
NR 120
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE
PI ABINGDON
PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND
BN 978-1-62958-385-3; 978-1-315-52893-9; 978-1-62958-384-6
J9 WAC RES H ARCHAEOL
PY 2016
BP 94
EP 106
PG 13
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA BG4IX
UT WOS:000388884300009
ER
PT B
AU Mulhern, DM
AF Mulhern, Dawn M.
BE Blau, S
Ubelaker, DH
TI Differentiating Human from Nonhuman Skeletal Remains
SO HANDBOOK OF FORENSIC ANTHROPOLOGY AND ARCHAEOLOGY, 2ND EDITION
SE World Archaeological Congress Research Handbooks in Archaeology
LA English
DT Article; Book Chapter
ID COMPACT-BONE TISSUE; SPECIES IDENTIFICATION; HAVERSIAN SYSTEMS; CORTICAL
BONE; HUMAN-ORIGIN; FRAGMENTS; AGE; MICROSTRUCTURE; MAMMALS; DNA
C1 [Mulhern, Dawn M.] Ft Lewis Coll, Anthropol, Durango, CO 81301 USA.
[Mulhern, Dawn M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Mulhern, Dawn M.] Disaster Mortuary Operat Response Team DMORT, Washington, DC USA.
RP Mulhern, DM (reprint author), Ft Lewis Coll, Anthropol, Durango, CO 81301 USA.; Mulhern, DM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.; Mulhern, DM (reprint author), Disaster Mortuary Operat Response Team DMORT, Washington, DC USA.
NR 63
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE
PI ABINGDON
PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND
BN 978-1-62958-385-3; 978-1-315-52893-9; 978-1-62958-384-6
J9 WAC RES H ARCHAEOL
PY 2016
BP 197
EP 212
PG 16
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA BG4IX
UT WOS:000388884300016
ER
PT B
AU Ross, AH
Kimmerle, EH
AF Ross, Ann H.
Kimmerle, Erin H.
BE Blau, S
Ubelaker, DH
TI Contribution of Quantitative Methods in Forensic Anthropology A New Era
SO HANDBOOK OF FORENSIC ANTHROPOLOGY AND ARCHAEOLOGY, 2ND EDITION
SE World Archaeological Congress Research Handbooks in Archaeology
LA English
DT Article; Book Chapter
ID GEOMETRIC MORPHOMETRIC-ANALYSIS; SEXUAL-DIMORPHISM; AGE ESTIMATION;
PHYSICAL-ANTHROPOLOGY; TECHNICAL NOTE; LONG BONES; IDENTIFICATION;
STATURE; DEATH; AMERICAN
C1 [Ross, Ann H.] North Carolina State Univ, Anthropol, Raleigh, NC 27695 USA.
[Kimmerle, Erin H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Kimmerle, Erin H.] Univ S Florida, Dept Anthropol, Tampa, FL USA.
RP Ross, AH (reprint author), North Carolina State Univ, Anthropol, Raleigh, NC 27695 USA.
NR 76
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE
PI ABINGDON
PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND
BN 978-1-62958-385-3; 978-1-315-52893-9; 978-1-62958-384-6
J9 WAC RES H ARCHAEOL
PY 2016
BP 622
EP 634
PG 13
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA BG4IX
UT WOS:000388884300043
ER
PT B
AU Blau, S
Ubelaker, DH
AF Blau, Soren
Ubelaker, Douglas H.
BE Blau, S
Ubelaker, DH
TI Conclusion International Perspectives on Issues in Forensic Anthropology
SO HANDBOOK OF FORENSIC ANTHROPOLOGY AND ARCHAEOLOGY, 2ND EDITION
SE World Archaeological Congress Research Handbooks in Archaeology
LA English
DT Editorial Material; Book Chapter
C1 [Blau, Soren] Victorian Inst Forens Med, Southbank, Vic, Australia.
[Blau, Soren] Monash Univ, Dept Forens Med, Clayton, Vic, Australia.
[Blau, Soren] Royal Coll Pathologists Australasia, Fac Sci, Surry Hills, NSW, Australia.
[Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Ubelaker, Douglas H.] George Washington Univ, Washington, DC 20052 USA.
[Ubelaker, Douglas H.] Michigan State Univ, E Lansing, MI 48824 USA.
[Ubelaker, Douglas H.] Amer Acad Forens Sci, Colorado Springs, CO USA.
RP Blau, S (reprint author), Victorian Inst Forens Med, Southbank, Vic, Australia.; Blau, S (reprint author), Monash Univ, Dept Forens Med, Clayton, Vic, Australia.; Blau, S (reprint author), Royal Coll Pathologists Australasia, Fac Sci, Surry Hills, NSW, Australia.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ROUTLEDGE
PI ABINGDON
PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND
BN 978-1-62958-385-3; 978-1-315-52893-9; 978-1-62958-384-6
J9 WAC RES H ARCHAEOL
PY 2016
BP 672
EP 677
PG 6
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA BG4IX
UT WOS:000388884300047
ER
EF