FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Cady, E
Prada, CM
An, X
Balasubramanian, K
Diaz, R
Kasdin, NJ
Kern, B
Kuhnert, A
Nemati, B
Poberezhskiy, I
Riggs, AJE
Zimmer, R
Zimmerman, N
AF Cady, Eric
Prada, Camilo Mejia
An, Xin
Balasubramanian, Kunjithapatham
Diaz, Rosemary
Kasdin, N. Jeremy
Kern, Brian
Kuhnert, Andreas
Nemati, Bijan
Poberezhskiy, Ilya
Riggs, A. J. Eldorado
Zimmer, Robert
Zimmerman, Neil
TI Demonstration of high contrast with an obscured aperture with the
WFIRST-AFTA shaped pupil coronagraph
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE high contrast imaging; coronagraphy; shaped pupil; exoplanets; wide
field infrared survey telescope-astrophysics-focused telescope asset
ID LYOT
AB The coronagraph instrument on the Wide-Field Infrared Survey Telescope-Astrophysics-Focused Telescope Asset (WFIRST-AFTA) mission study has two coronagraphic architectures, shaped pupil and hybrid Lyot, which may be interchanged for use in different observing scenarios. Each architecture relies on newly developed mask components to function in the presence of the AFTA aperture, and so both must be matured to a high technology readiness level in advance of the mission. A series of milestones were set to track the development of the technologies required for the instrument; we report on completion of WFIRST-AFTA coronagraph milestone 2-a narrowband 10-8 contrast test with static aberrations for the shaped pupil-and the plans for the upcoming broadband coronagraph milestone 5. (c) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Cady, Eric; Prada, Camilo Mejia; An, Xin; Balasubramanian, Kunjithapatham; Diaz, Rosemary; Kern, Brian; Kuhnert, Andreas; Nemati, Bijan; Poberezhskiy, Ilya; Zimmer, Robert] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kasdin, N. Jeremy; Riggs, A. J. Eldorado; Zimmerman, Neil] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
RP Cady, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM eric.j.cady@jpl.nasa.gov
OI Riggs, A J Eldorado/0000-0002-0863-6228
NR 23
TC 3
Z9 3
U1 1
U2 1
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011004
DI 10.1117/1.JATIS.2.1.011004
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200005
ER
PT J
AU Groff, TD
Riggs, AJE
Kern, B
Kasdin, NJ
AF Groff, Tyler D.
Riggs, A. J. Eldorado
Kern, Brian
Kasdin, N. Jeremy
TI Methods and limitations of focal plane sensing, estimation, and control
in high-contrast imaging
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE aberrations; wavefront compensation; wavefront sensors; wavefronts;
signal detection; Fourier optics
ID ABERRATIONS; CORONAGRAPH; PUPIL
AB Coronagraphy is a very promising method for directly imaging exoplanets, but the performance of a coronagraph is highly sensitive to quasi-static aberrations within the telescope. The resultant speckles are suppressed in the final focal plane using a wavefront control system that estimates the field at the final focal plane to avoid any noncommon path error. This requires a set of probe images that modulate the field so that it may be estimated. With an estimate of the focal plane electric field, a control law is defined to suppress the speckle field so that the planet can be imaged. Characterizing the planet requires that the speckle field be suppressed simultaneously over the bandpass of interest. The choice of control law, bandpass, estimator, and probing methodology has implications in the control solutions and contrast performance. Here, we compare wavefront probing, estimation, and control algorithms, and describe their practical implementation. (c) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Groff, Tyler D.; Riggs, A. J. Eldorado; Kasdin, N. Jeremy] Princeton Univ, Dept Mech & Aerosp Engn, Equad Olden St, Princeton, NJ 08544 USA.
[Kern, Brian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Groff, TD (reprint author), Princeton Univ, Dept Mech & Aerosp Engn, Equad Olden St, Princeton, NJ 08544 USA.
EM tgroff@princeton.edu
OI Riggs, A J Eldorado/0000-0002-0863-6228
NR 29
TC 8
Z9 8
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011009
DI 10.1117/1.JATIS.2.1.011009
PG 15
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200010
ER
PT J
AU Harding, LK
Demers, RT
Hoenk, M
Peddada, P
Nemati, B
Cherng, M
Michaels, D
Neat, LS
Loc, A
Bush, N
Hall, D
Murray, N
Gow, J
Burgon, R
Holland, A
Reinheimer, A
Jorden, PR
Jordan, D
AF Harding, Leon K.
Demers, Richard T.
Hoenk, Michael
Peddada, Pavani
Nemati, Bijan
Cherng, Michael
Michaels, Darren
Neat, Leo S.
Loc, Anthony
Bush, Nathan
Hall, David
Murray, Neil
Gow, Jason
Burgon, Ross
Holland, Andrew
Reinheimer, Alice
Jorden, Paul R.
Jordan, Douglas
TI Technology advancement of the CCD201-20 EMCCD for the WFIRST coronagraph
instrument: sensor characterization and radiation damage
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE electron multiplying charge-coupled devices; WFIRST-AFTA; radiation
damage; L2 orbit; techniques: mitigation
ID DISPLACEMENT DAMAGE; SILICON; INTENSIFIER; TELESCOPE; DEVICES; CAMERA;
MODEL; CCDS
AB The Wide Field InfraRed Survey Telescope-Astrophysics Focused Telescope Asset (WFIRST-AFTA) mission is a 2.4-m class space telescope that will be used across a swath of astrophysical research domains. JPL will provide a high-contrast imaging coronagraph instrument-one of two major astronomical instruments. In order to achieve the low noise performance required to detect planets under extremely low flux conditions, the electron multiplying charge-coupled device (EMCCD) has been baselined for both of the coronagraph's sensors-the imaging camera and integral field spectrograph. JPL has established an EMCCD test laboratory in order to advance EMCCD maturity to technology readiness level-6. This plan incorporates full sensor characterization, including read noise, dark current, and clock-induced charge. In addition, by considering the unique challenges of the WFIRST space environment, degradation to the sensor's charge transfer efficiency will be assessed, as a result of damage from high-energy particles such as protons, electrons, and cosmic rays. Science-grade CCD201-20 EMCCDs have been irradiated to a proton fluence that reflects the projected WFIRST orbit. Performance degradation due to radiation displacement damage is reported, which is the first such study for a CCD201-20 that replicates the WFIRST conditions. In addition, techniques intended to identify and mitigate radiation-induced electron trapping, such as trap pumping, custom clocking, and thermal cycling, are discussed. (c) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Harding, Leon K.; Demers, Richard T.; Hoenk, Michael; Peddada, Pavani; Nemati, Bijan; Cherng, Michael; Michaels, Darren; Neat, Leo S.; Loc, Anthony] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bush, Nathan; Hall, David; Murray, Neil; Gow, Jason; Burgon, Ross; Holland, Andrew] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Reinheimer, Alice] E2v Inc, 765 Sycamore Dr, Milpitas, CA 95035 USA.
[Jorden, Paul R.; Jordan, Douglas] E2v Technol, 106 Waterhouse Lane, Chelmsford CM1 2QU, Essex, England.
RP Harding, LK; Demers, RT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Leon.K.Harding@jpl.nasa.gov; Richard.T.Demers@jpl.nasa.gov
NR 54
TC 8
Z9 8
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011007
DI 10.1117/1.JATIS.2.1.011007
PG 31
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200008
ER
PT J
AU Hicks, BA
AF Hicks, Brian A.
TI Exoplanet detection and characterization via parallel broadband nulling
coronagraphy
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE coronagraphy; nulling interferometers; exoplanets; spectroimagers
ID ACHROMATIC PHASE SHIFTERS; EXTRASOLAR PLANET; INTERFEROMETRY; EARTH;
STARS
AB The contrast and angular resolution required to directly image and characterize mature exoplanetary systems place stringent requirements on the space-based telescopes and starlight suppression systems needed to study spatial distributions of debris disks, exozodiacal dust, and individual planets at multiple epochs in their orbits. A nulling interferometer (nuller) is a coronagraphic suppression system that can be used with all telescope types, including those with obscured and segmented apertures envisioned for upcoming and future observatories. One of the challenges for detection and characterization of exoplanetary signals is achieving high contrast with broad spectral coverage. This work presents design concepts for broadband nulling over four parallel similar to 20% bandpasses spanning the visible spectrum. Contrast-limiting effects of stellar angular extent, residual chromaticity of broadband phase shifters, and aperture diffraction are considered to reach simultaneous less than or similar to 2 x 10(-8) contrast over separations spanning 0.2 to 0.9 arc sec for a 2.4-m telescope observing a Sun-like star at 10 pc. With added dark hole wavefront control and postprocessing point spread function subtraction techniques to further reduce scattered starlight, such a system could be capable of detecting the very the nearest Earthlike exoplanets and spectral characterization of several nearby extrasolar gas giants. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Hicks, Brian A.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Hicks, BA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM brian.a.hicks@nasa.gov
NR 32
TC 2
Z9 2
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011015
DI 10.1117/1.JATIS.2.1.011015
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200016
ER
PT J
AU Kern, B
AF Kern, Brian
TI Impact of WFIRST-AFTA line-of-sight jitter distributions on
phase-induced amplitude apodization complex mask coronagraph science
yield
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE coronagraph; exoplanets; wavefront control
AB A framework for evaluating the science yield of a coronagraph in the presence of a variety of line-of-sight jitter environments is described and the use of a tip-tilt threshold for improving science yield is proposed. The current expectations of the WFIRST-AFTA mission are used for specific distributions of line-of-sight jitter, including the current expectations for tip-tilt correction using a low-order wavefront sensor/control. The effect of the residual tip-tilt on the phase-induced amplitude apodization complex mask coronagraph (PIAACMC) architecture is considered, because the performance of the PIAACMC architecture is expected to be dominated by tip-tilt sensitivity, implying that this treatment has a large impact on the final science yield. The most important outcomes of this study are that the rms residual tip-tilt expected after correction is 0.6 mas rms/axis and that by eliminating some science frames during analysis through a tip-tilt threshold, the number of planets observable increases by similar to 25% for the 550-nm imaging channel. The number of known radial velocity planets expected to be observed ranges from 29 to 78 at 550 nm and from 9 to 12 at 890 nm. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Kern, Brian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91016 USA.
RP Kern, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91016 USA.
EM Brian.D.Kern@jpl.nasa.gov
NR 9
TC 3
Z9 3
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011016
DI 10.1117/1.JATIS.2.1.011016
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200017
ER
PT J
AU Kern, B
Guyon, O
Belikov, R
Wilson, D
Muller, R
Sidick, E
Balasubramanian, B
Krist, J
Poberezhskiy, I
Tang, H
AF Kern, Brian
Guyon, Olivier
Belikov, Ruslan
Wilson, Daniel
Muller, Richard
Sidick, Erkin
Balasubramanian, Bala
Krist, John
Poberezhskiy, Ilya
Tang, Hong
TI Phase-induced amplitude apodization complex mask coronagraph mask
fabrication, characterization, and modeling for WFIRST-AFTA
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE coronagraph; exoplanets; wavefront control
AB This work describes the fabrication, characterization, and modeling of a second-generation occulting mask for a phase-induced amplitude apodization complex mask coronagraph, designed for use on the WFIRST-AFTA mission. The mask has many small features (similar to micron lateral scales) and was fabricated at the Jet Propulsion Laboratory Microdevices Laboratory, then characterized using a scanning electron microscope, atomic force microscope, and optical interferometric microscope. The measured fabrication errors were then fed to a wavefront control model which predicts the contrast performance of a full coronagraph. The expected coronagraphic performance using this mask is consistent with observing similar to 15 planetary targets with WFIRST-AFTA in a reasonable time (<1 day/target). (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Kern, Brian; Wilson, Daniel; Muller, Richard; Sidick, Erkin; Balasubramanian, Bala; Krist, John; Poberezhskiy, Ilya; Tang, Hong] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91016 USA.
[Guyon, Olivier] Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Guyon, Olivier] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Guyon, Olivier] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Belikov, Ruslan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kern, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91016 USA.
EM Brian.D.Kern@jpl.nasa.gov
NR 10
TC 4
Z9 4
U1 2
U2 2
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR UNSP 011014
DI 10.1117/1.JATIS.2.1.011014
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200015
ER
PT J
AU Krist, J
Nemati, B
Mennesson, B
AF Krist, John
Nemati, Bijan
Mennesson, Bertrand
TI Numerical modeling of the proposed WFIRST-AFTA coronagraphs and their
predicted performances
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE Wide Field Infrared Survey Telescope; Astrophysics Focused Telescope
Asset; coronagraph
ID HUBBLE-SPACE-TELESCOPE; PIAA CORONAGRAPHY; CONTRAST; LYOT
AB The WFIRST-AFTA 2.37 m telescope will provide the opportunity to host a coronagraph for the imaging and spectroscopy of planets and disks in the next decade. The telescope, however, is not ideal, given its obscured aperture. Only recently have coronagraph designs been thoroughly investigated that can efficiently work with this configuration. Three coronagraph designs, the hybrid Lyot, shaped pupil, and phase-induced amplitude apodization complex mask coronagraph have been selected for further development by the Astrophysics Focused Telescope Asset project. Real-world testbed demonstrations of these have just begun, so for now, the most reliable means of evaluating their potential performance comes from numerical modeling incorporating diffraction propagation, realistic system models, and simulated wavefront sensing and control. Here, we present the methods of performance evaluation and results for the current coronagraph designs. (c) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Krist, John; Nemati, Bijan; Mennesson, Bertrand] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Krist, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM john.krist@jpl.nasa.gov
NR 41
TC 8
Z9 8
U1 3
U2 5
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011003
DI 10.1117/1.JATIS.2.1.011003
PG 26
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200004
ER
PT J
AU Noecker, MC
Zhao, F
Demers, R
Trauger, J
Guyon, O
Kasdin, NJ
AF Noecker, M. Charley
Zhao, Feng
Demers, Rick
Trauger, John
Guyon, Olivier
Kasdin, N. Jeremy
TI Coronagraph instrument for WFIRST-AFTA
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE astronomy; space telescope; exoplanet; coronagraph; WFIRST-AFTA
ID COMPANION
AB The Wide-Field Infrared Survey Telescope (WFIRST) is a NASA observatory concept, now in phase A study, which is designed to perform wide-field imaging and slitless spectroscopic surveys for dark energy research and other astrophysical studies. It will also perform microlensing surveys to look for distant exoplanets in our galaxy, and direct imaging studies of some of the very nearest exoplanets. The current astrophysics focused telescope assets (AFTA) design of the mission makes use of an existing 2.4-m telescope, which yields enhanced sensitivity and imaging performance in all these science programs. AFTA also enables the addition of a coronagraph instrument (CGI) for direct imaging and spectroscopy of nearby giant exoplanets (including some that were discovered by radial velocity and other methods), and also for observing debris disks around the candidate host stars. This paper outlines the context for the other papers in this special volume on the WFIRST-AFTA CGI, covering the science, design, engineering, and technology development of the observatory and its CGI. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Noecker, M. Charley; Zhao, Feng; Demers, Rick; Trauger, John] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Guyon, Olivier] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Plane, Hilo, HI 96720 USA.
[Guyon, Olivier] Univ Arizona, UAz Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Kasdin, N. Jeremy] Princeton Univ, C234 Engn Quadrangle, Princeton, NJ 08544 USA.
RP Noecker, MC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM charley.noecker@jpl.nasa.gov
NR 20
TC 6
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U1 3
U2 3
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR UNSP 011001
DI 10.1117/1.JATIS.2.1.011001
PG 6
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200002
ER
PT J
AU Pluzhnik, E
Guyon, O
Belikov, R
Bendek, E
AF Pluzhnik, Eugene
Guyon, Olivier
Belikov, Ruslan
Bendek, Eduardo
TI Design of off-axis mirrors for the phase-induced amplitude apodization
complex mask coronagraph
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE exoplanets; coronagraphy; phase-induced amplitude apodization; optical
design
AB The phase-induced amplitude apodization complex mask coronagraph (PIAACMC) provides an efficient way to control diffraction propagation effects caused by the central obstruction/segmented mirrors of the telescope. PIAACMC can be optimized in a way that takes into account both chromatic diffraction effects caused by the telescope obstructed aperture and the tip-tilt sensitivity of the coronagraph. As a result, unlike classic phase-induced amplitude apodization (PIAA), the PIAACMC mirror shapes are often slightly asymmetric even for an on-axis configuration and require more care in calculating off-axis shapes when an off-axis configuration is preferred. A method to design off-axis PIAA mirror shapes given an on-axis mirror design is presented. The algorithm is based on geometrical ray tracing and is able to calculate off-axis PIAA mirror shapes for an arbitrary geometry of the input and output beams. The method is demonstrated using the third generation PIAACMC design for WFIRST-AFTA telescope. Geometrical optics design issues related to the off-axis diffraction propagation effects are also discussed. (c) The Authors.
C1 [Pluzhnik, Eugene; Belikov, Ruslan; Bendek, Eduardo] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guyon, Olivier] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Guyon, Olivier] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
RP Pluzhnik, E (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM yevgeniy.a.pluzhnyk@nasa.gov
NR 9
TC 2
Z9 2
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR UNSP 011018
DI 10.1117/1.JATIS.2.1.011018
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200019
ER
PT J
AU Seo, BJ
Gordon, B
Kern, B
Kuhnert, A
Moody, D
Muller, R
Poberezhskiy, I
Trauger, J
Wilson, D
AF Seo, Byoung-Joon
Gordon, Brian
Kern, Brian
Kuhnert, Andy
Moody, Dwight
Muller, Richard
Poberezhskiy, Ilya
Trauger, John
Wilson, Daniel
TI Hybrid Lyot coronagraph for wide-field infrared survey
telescope-astrophysics focused telescope assets: occulter fabrication
and high contrast narrowband testbed demonstration
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE hybrid Lyot coronagraph; high contrast imaging; deformable mirror;
astrophysics focused telescope assets wide-field infrared survey
telescope; stellar coronagraph; exoplanet direct imaging
ID ELECTRON-BEAM LITHOGRAPHY
AB Hybrid Lyot coronagraph (HLC) is one of the two operating modes of the WFIRST-AFTA coronagraph instrument. It produces starlight suppression over the full 360-deg annular region and thus is particularly suitable to improve the discovery space around WFIRST-AFTA targets. Since being selected by the National Aeronautics and Space Administration in December 2013, the coronagraph technology is being matured to technology readiness level 5 by September 2016. We present the progress of HLC key component fabrication and testbed demonstrations with the WFIRST-AFTA pupil. For the first time, a circular HLC occulter mask consisting of metal and dielectric layers is fabricated and characterized. Wavefront control using two deformable mirrors is successfully demonstrated in a vacuum testbed with narrowband light (<1-nm bandwidth at 516 nm) to obtain repeatable convergence below 8 x 10(-9) mean contrast in the 360-deg dark hole with a working angle between 3 lambda/D and 9 lambda/D with arbitrary polarization. We detail the hardware and software used in the testbed, the results, and the associated analysis. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Seo, Byoung-Joon; Gordon, Brian; Kern, Brian; Kuhnert, Andy; Moody, Dwight; Muller, Richard; Poberezhskiy, Ilya; Trauger, John; Wilson, Daniel] CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Seo, BJ (reprint author), CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Byoung-Joon.Seo@jpl.nasa.gov
NR 18
TC 0
Z9 0
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011019
DI 10.1117/1.JATIS.2.1.011019
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200020
ER
PT J
AU Shi, F
Balasubramanian, K
Hein, R
Lam, R
Moore, D
Moore, J
Patterson, K
Poberezhskiy, I
Shields, J
Sidick, E
Tang, H
Truong, T
Wallace, JK
Wang, X
Wilson, D
AF Shi, Fang
Balasubramanian, Kunjithapatham
Hein, Randall
Lam, Raymond
Moore, Douglas
Moore, James
Patterson, Keith
Poberezhskiy, Ilya
Shields, Joel
Sidick, Erkin
Tang, Hong
Tuan Truong
Wallace, J. Kent
Wang, Xu
Wilson, Daniel
TI Low-order wavefront sensing and control for WFIRST-AFTA coronagraph
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE wavefront sensing and control; stellar coronagraph; Wide-Field Infrared
Survey Telescope
ID ADAPTIVE OPTICS; SENSOR; CALIBRATION; PRINCIPLE
AB To maintain the required Wide-Field Infrared Survey Telescope (WFIRST) coronagraph performance in a realistic space environment, a low-order wavefront sensing and control (LOWFS/C) subsystem is necessary. The LOWFS/C uses the rejected stellar light from the coronagraph to sense and suppress the telescope pointing errors as well as low-order wavefront errors (WFEs) due to changes in thermal loading of the telescope and the rest of the observatory. We will present a conceptual design of a LOWFS/C subsystem for the WFIRST-AFTA coronagraph. This LOWFS/C uses a Zernike phase contrast wavefront sensor (ZWFS) with a phase shifting disk combined with the stellar light rejecting occulting masks, a key concept to minimize the noncommon path error. We will present our analysis of the sensor performance and evaluate the performance of the line-of-sight jitter suppression loop, as well as the low-order WFE correction loop with a deformable mirror on the coronagraph. We will also report the LOWFS/C testbed design and the preliminary in-air test results, which show a very promising performance of the ZWFS. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Shi, Fang; Balasubramanian, Kunjithapatham; Hein, Randall; Lam, Raymond; Moore, Douglas; Moore, James; Patterson, Keith; Poberezhskiy, Ilya; Shields, Joel; Sidick, Erkin; Tang, Hong; Tuan Truong; Wallace, J. Kent; Wang, Xu; Wilson, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA.
RP Shi, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA.
EM Fang.Shi@jpl.nasa.gov
NR 31
TC 1
Z9 1
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011021
DI 10.1117/1.JATIS.2.1.011021
PG 19
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200022
ER
PT J
AU Traub, WA
Breckinridge, J
Greene, TP
Guyon, O
Kasdin, NJ
Macintosh, B
AF Traub, Wesley A.
Breckinridge, James
Greene, Thomas P.
Guyon, Olivier
Kasdin, N. Jeremy
Macintosh, Bruce
TI Science yield estimate with the Wide-Field Infrared Survey Telescope
coronagraph
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE coronagraphs; exoplanets; direct imaging; spectra; disks
ID MAIN-SEQUENCE STARS; EXOPLANETS; COLORS
AB The coronagraph instrument (CGI) on the Wide-Field Infrared Survey Telescope will directly image and spectrally characterize planets and circumstellar disks around nearby stars. Here we estimate the expected science yield of the CGI for known radial-velocity (RV) planets and potential circumstellar disks. The science return is estimated for three types of coronagraphs: the hybrid Lyot and shaped pupil are the currently planned designs, and the phase-induced amplitude apodizing complex mask coronagraph is the backup design. We compare the potential performance of each type for imaging as well as spectroscopy. We find that the RV targets can be imaged in sufficient numbers to produce substantial advances in the science of nearby exoplanets. To illustrate the potential for circumstellar disk detections, we estimate the brightness of zodiacal-type disks, which could be detected simultaneously during RV planet observations. (c) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Traub, Wesley A.] CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Breckinridge, James] CALTECH, M-S 105-50,1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Greene, Thomas P.] NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
[Guyon, Olivier] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Guyon, Olivier] Univ Arizona, Coll Opt Sci, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Kasdin, N. Jeremy] Princeton Univ, C234 Engn Quadrangle, Princeton, NJ 08544 USA.
[Macintosh, Bruce] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Varian Phys Bldg,382 Via Pueblo Mall, Stanford, CA 94305 USA.
RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM wtraub@jpl.nasa.gov
NR 33
TC 6
Z9 6
U1 1
U2 2
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011020
DI 10.1117/1.JATIS.2.1.011020
PG 17
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200021
ER
PT J
AU Trauger, J
Moody, D
Krist, J
Gordon, B
AF Trauger, John
Moody, Dwight
Krist, John
Gordon, Brian
TI Hybrid Lyot coronagraph for WFIRST-AFTA: coronagraph design and
performance metrics
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE exoplanet; coronagraph; active optics
AB The prospect of extreme high-contrast astronomical imaging from space has inspired developments of new coronagraph methods for exoplanet imaging and spectroscopy. However, the requisite imaging contrast, at levels of 1 billion to one or better for the direct imaging of cool mature exoplanets in reflected visible starlight, leads to challenging new requirements on the stability and control of the optical wavefront, at levels currently beyond the reach of ground-based telescopes. We review the design, performance, and science prospects for the hybrid Lyot coronagraph (HLC) on the WFIRST-AFTA telescope. Together with a pair of deformable mirrors for active wavefront control, the HLC creates a full 360-deg high-contrast dark field of view at 10(-9) contrast levels or better, extending to within angular separations of 3 lambda(0)/D from the central star, over spectral bandwidths of 10% or more. (c) The Authors.
C1 [Trauger, John; Moody, Dwight; Krist, John; Gordon, Brian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Trauger, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM john.trauger@jpl.nasa.gov
NR 25
TC 11
Z9 11
U1 2
U2 2
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2016
VL 2
IS 1
AR 011013
DI 10.1117/1.JATIS.2.1.011013
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DJ4QM
UT WOS:000374192200014
ER
PT B
AU Lee, DE
Nesmith, B
Hendricks, T
Cepeda-Rizo, J
Petach, M
Tward, E
Penera, C
Pohner, J
Whitney, S
Grandidier, J
AF Lee, David E.
Nesmith, Bill
Hendricks, Terry
Cepeda-Rizo, Juan
Petach, Michael
Tward, Emanuel
Penera, Cecilia
Pohner, John
Whitney, Scott
Grandidier, Jonathan
GP ASME
TI EFFICIENT HEAT TRANSFER METHODS IN A HYBRID SOLAR THERMAL POWER SYSTEM
FOR THE FSPOT-X PROJECT
SO PROCEEDINGS OF THE ASME 9TH INTERNATIONAL CONFERENCE ON ENERGY
SUSTAINABILITY, 2015, VOL 1
LA English
DT Proceedings Paper
CT 9th ASME International Conference on Energy Sustainability
CY JUN 28-JUL 02, 2015
CL San Diego, CA
SP ASME, Adv Energy Syst Div, ASME, Solar Energy Div
AB The FSPOT-X Project, focused on maximizing exergy generated from AM1.5 sunlight, targets an overall system efficiency of >35%. The objective hybrid power system will deliver grid-ready AC power while simultaneously providing thermal energy storage for dispatchable electrical power generation in post sunset conditions. The challenging system level requirements flow-down critical temperature differential and thermal transport requirements to multiple system components and their interfaces. By integrating and demonstrating multiple technologies, the FSPOT-X hybrid power system seeks to efficiently convert photons to electrons maximizing heat transfer efficiency across system element interfaces. These include: I1) capturing all incident sunlight from the solar concentrator in a receiver cavity to maximize energy generation from the CPV cells, 12) extracting PV thermalization heat from the receiver and into the reflux chamber, 13) moving heat from the reflux chamber through the thermal transfer interface, 14) using the thermal transfer interface to shift heat into the TAPC's hot heat exchanger, 15) storing excess unused heat in phase change material, and 16) disposal of waste heat at the system level. For each of these thermal interfaces, effective and efficient technical means are being used and applied in order to maximize overall system efficiency for delivery of a next generation cost-effective and market-ready solar power system.
C1 [Lee, David E.; Petach, Michael; Tward, Emanuel; Penera, Cecilia; Pohner, John; Whitney, Scott] Northrop Grumman Aerosp Syst, Redondo Beach, CA USA.
[Nesmith, Bill; Hendricks, Terry; Cepeda-Rizo, Juan; Grandidier, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Lee, DE (reprint author), Northrop Grumman Aerosp Syst, Redondo Beach, CA USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5684-0
PY 2016
AR V001T03A005
PG 7
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels
SC Science & Technology - Other Topics; Energy & Fuels
GA BE6KS
UT WOS:000374279400017
ER
PT J
AU Kumar-Krishnan, S
Hernandez-Rangel, A
Pal, U
Ceballos-Sanchez, O
Flores-Ruiz, FJ
Prokhorov, E
de Fuentes, OA
Esparza, R
Meyyappan, M
AF Kumar-Krishnan, Siva
Hernandez-Rangel, A.
Pal, Umapada
Ceballos-Sanchez, O.
Flores-Ruiz, F. J.
Prokhorov, E.
Arias de Fuentes, O.
Esparza, Rodrigo
Meyyappan, M.
TI Surface functionalized halloysite nanotubes decorated with silver
nanoparticles for enzyme immobilization and biosensing
SO JOURNAL OF MATERIALS CHEMISTRY B
LA English
DT Article
ID DIRECT ELECTRON-TRANSFER; WALLED CARBON NANOTUBES; GLUCOSE-OXIDASE; GOLD
NANOPARTICLE; REDOX ENZYMES; BIOFUEL CELLS; IONIC LIQUID; PLATFORM;
NANOTECHNOLOGY; NANOCOMPOSITE
AB Improving enzyme immobilization with high loading capacity and achieving direct electron transfer (DET) between the enzyme and the electrode surface is key to designing highly sensitive enzymatic electrochemical biosensors. Herein, we report a novel approach based on the selective modification of the outer surface of halloysite nanotubes (HNTs) that supports silver nanoparticles (AgNPs) to obtain a hybrid nanocomposite. AgNPs of about 10 nm average size could be uniformly supported on silane-modified HNTs through in situ reduction of Ag+ ions. The resultant nanocomposite shows an excellent support capability for the effective immobilization and electrical wiring of redox enzyme glucose oxidase (GOx). The GOx immobilized HNT/AgNPs were deposited on the glassy carbon electrode (GCE) and utilized for the bioelectrocatalyzed electrochemical detection of glucose. The GOx modified composite electrodes show glucose sensitivity as high as 5.1 mu A mM(-1) cm(-2), which is higher than for the electrodes prepared without surface functionalization.
C1 [Kumar-Krishnan, Siva; Esparza, Rodrigo] Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Santiago De Queretaro 76230, Qro, Mexico.
[Hernandez-Rangel, A.; Prokhorov, E.; Arias de Fuentes, O.] Cinvestav Queretaro, Queretaro 76230, Qro, Mexico.
[Pal, Umapada] Benemerita Univ Autonoma Puebla, Inst Fis, Puebla 72570, Mexico.
[Ceballos-Sanchez, O.] UANL, Dept Ecomat & Energia, Fac Ingn Civil, Catedras Conacyt, San Nicolas De Los Garza 64451, Nuevo Leon, Mexico.
[Flores-Ruiz, F. J.] UNAM, Ctr Nanociencias & Nanotecnol, Ensenada 22860, BC, Mexico.
[Arias de Fuentes, O.] Univ La Habana, Inst Ciencia & Tecnol Mat, Havana 10400, Cuba.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kumar-Krishnan, S (reprint author), Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Blvd Juriquilla 3001, Santiago De Queretaro 76230, Qro, Mexico.
EM skumar@fata.unam.mx
RI UANL, FIC-UANL/O-5444-2015; Flores-Ruiz, Francisco /D-5089-2017
OI Flores-Ruiz, Francisco /0000-0002-8445-4223
FU DGAPA-UNAM post-doctoral fellowship
FX This work was supported by the DGAPA-UNAM post-doctoral fellowship. The
authors are grateful to J. A. Munoz-Salas for assistance with the
construction of the GCE electrodes, Ma. Lourdes Palma Tirado (Campus
UNAM Juriquilla, Qro), for TEM measurements.
NR 58
TC 3
Z9 3
U1 28
U2 52
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2050-750X
EI 2050-7518
J9 J MATER CHEM B
JI J. Mat. Chem. B
PY 2016
VL 4
IS 15
BP 2553
EP 2560
DI 10.1039/c6tb00051g
PG 8
WC Materials Science, Biomaterials
SC Materials Science
GA DJ3IS
UT WOS:000374098800004
ER
PT J
AU Huang, FT
Mayr, HG
Russell, JM
Mlynczak, MG
AF Huang, F. T.
Mayr, H. G.
Russell, J. M., III
Mlynczak, M. G.
TI Ozone and temperature decadal responses to solar variability in the
mesosphere and lower thermosphere, based on measurements from SABER on
TIMED
SO ANNALES GEOPHYSICAE
LA English
DT Article
DE Meteorology and atmospheric dynamics; climatology
ID LONG-TERM; FORT-COLLINS; STRATOSPHERE; TRENDS; MODEL
AB We have derived ozone and temperature responses to solar variability over a solar cycle, from June 2002 through June 2014, 50 to 100aEuro-km, 48A degrees aEuro-S to 48A degrees aEuro-N, based on data from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the Thermosphere-Ionosphere-Mesosphere-Energetics and Dynamics (TIMED) satellite. Results with this extent of coverage in the mesosphere and lower thermosphere have not been available previously. A multiple regression is applied to obtain responses as a function of the solar 10.7aEuro-cm flux (solar flux units, sfu). Positive responses mean that they are larger at solar maximum than at solar minimum of the solar cycle. From similar to aEuro parts per thousand aEuro-80 to 100aEuro-km, both ozone and temperature responses are positive for all latitudes and are larger than those at lower altitudes. From similar to aEuro parts per thousand aEuro-80 to 100aEuro-km, ozone responses can exceed 10aEuro-%aEuro-(100aEuro-sfu)(-1), and temperature responses can approach 4aEuro-A degrees K. From 50 to similar to aEuro parts per thousand aEuro-80aEuro-km, the ozone responses at low latitudes ( similar to similar to aEuro parts per thousand aEuro-A +/- 35A degrees) are mostly negative and can approach similar to aEuro parts per thousand aEuro-negative 3aEuro-%aEuro-(100aEuro-sfu)(-1). However, they are mostly positive at midlatitudes in this region and can approach similar to aEuro parts per thousand aEuro-2aEuro-%aEuro-(100aEuro-sfu)(-1). In contrast to ozone, from similar to aEuro parts per thousand aEuro-50 to 80aEuro-km, the temperature responses at low latitudes remain positive, with values up to similar to similar to aEuro parts per thousand aEuro-2.5aEuro-KaEuro-(100aEuro-sfu)(-1), but are weakly negative at midlatitudes. Consequently, there is a systematic and robust relation between the phases of the ozone and temperature responses. They are positively correlated (in phase) from similar to aEuro parts per thousand aEuro-80 to 100aEuro-km for all latitudes and negatively correlated (out of phase) from similar to aEuro parts per thousand aEuro-50 to 80aEuro-km, also for all latitudes. The negative correlation from 50 to 80aEuro-km is maintained even though the ozone and temperature responses can change signs as a function of altitude and latitude, because the corresponding temperature responses change signs in step with ozone. This is consistent with the idea that dynamics have the larger influence between similar to aEuro parts per thousand aEuro-80 and 100aEuro-km, while photochemistry is more in control from similar to aEuro parts per thousand aEuro-50 to 75aEuro-km. The correlation coefficients between the solar 10.7aEuro-cm flux and the ozone and temperature themselves from 2012 to 2014 are positive (negative) in regions where the responses are positive (negative). This supports our results since the correlations are independent of the multiple regression used to derive the responses. We also compare with previous results.
C1 [Huang, F. T.] Univ Maryland, Baltimore County, MD 21250 USA.
[Mayr, H. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Huang, FT (reprint author), Univ Maryland, Baltimore County, MD 21250 USA.
EM fthuang@verizon.net
NR 31
TC 2
Z9 2
U1 2
U2 7
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 0992-7689
EI 1432-0576
J9 ANN GEOPHYS-GERMANY
JI Ann. Geophys.
PY 2016
VL 34
IS 1
BP 29
EP 40
DI 10.5194/angeo-34-29-2016
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DI6GJ
UT WOS:000373596900003
ER
PT J
AU Palmerio, E
Kilpua, EKJ
Savani, NP
AF Palmerio, Erika
Kilpua, Emilia K. J.
Savani, Neel P.
TI Planar magnetic structures in coronal mass ejection-driven sheath
regions
SO ANNALES GEOPHYSICAE
LA English
DT Article
DE Interplanetary physics; interplanetary shocks; solar wind plasma; solar
physics astrophysics and astronomy; flares and mass ejections
ID SOLAR-WIND; INTERPLANETARY SHOCKS; FIELDS; EARTH; EVOLUTION; MAXIMUM;
CLOUDS; STORMS
AB Planar magnetic structures (PMSs) are periods in the solar wind during which interplanetary magnetic field vectors are nearly parallel to a single plane. One of the specific regions where PMSs have been reported are coronal mass ejection (CME)-driven sheaths. We use here an automated method to identify PMSs in 95 CME sheath regions observed in situ by the Wind and ACE spacecraft between 1997 and 2015. The occurrence and location of the PMSs are related to various shock, sheath, and CME properties. We find that PMSs are ubiquitous in CME sheaths; 85% of the studied sheath regions had PMSs with the mean duration of 6 h. In about one-third of the cases the magnetic field vectors followed a single PMS plane that covered a significant part (at least 67%) of the sheath region. Our analysis gives strong support for two suggested PMS formation mechanisms: the amplification and alignment of solar wind discontinuities near the CME-driven shock and the draping of the magnetic field lines around the CME ejecta. For example, we found that the shock and PMS plane normals generally coincided for the events where the PMSs occurred near the shock (68% of the PMS plane normals near the shock were separated by less than 20 degrees from the shock normal), while deviations were clearly larger when PMSs occurred close to the ejecta leading edge. In addition, PMSs near the shock were generally associated with lower upstream plasma beta than the cases where PMSs occurred near the leading edge of the CME. We also demonstrate that the planar parts of the sheath contain a higher amount of strong southward magnetic field than the non-planar parts, suggesting that planar sheaths are more likely to drive magnetospheric activity.
C1 [Palmerio, Erika; Kilpua, Emilia K. J.] Univ Helsinki, Dept Phys, POB 64, FIN-00014 Helsinki, Finland.
[Savani, Neel P.] Univ Maryland, GPHI, Baltimore, MD 21201 USA.
[Savani, Neel P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Palmerio, E (reprint author), Univ Helsinki, Dept Phys, POB 64, FIN-00014 Helsinki, Finland.
EM erika.palmerio@helsinki.fi
RI Kilpua, Emilia/G-8994-2012;
OI Palmerio, Erika/0000-0001-6590-3479
FU Magnus Ehrnrooth foundation; Academy of Finland [1267087]
FX We thank A. Szabo for the WIND MFI data, K. W. Ogilvie for the WIND SWE
data, N. Ness for the ACE magnetic field data and D. J. McComas for the
ACE SWE data. E. Palmerio acknowledges the Magnus Ehrnrooth foundation
for financial support. E. K. J. Kilpua acknowledges Academy of Finland
project 1267087 for financial support. This paper uses data from the
Heliospheric Shock Database, generated and maintained at the University
of Helsinki.
NR 38
TC 4
Z9 4
U1 0
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 0992-7689
EI 1432-0576
J9 ANN GEOPHYS-GERMANY
JI Ann. Geophys.
PY 2016
VL 34
IS 2
BP 313
EP 322
DI 10.5194/angeo-34-313-2016
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DI7XZ
UT WOS:000373716600014
ER
PT J
AU Maurice, S
Clegg, SM
Wiens, RC
Gasnault, O
Rapin, W
Forni, O
Cousin, A
Sautter, V
Mangold, N
Le Deit, L
Nachon, M
Anderson, RB
Lanza, NL
Fabre, C
Payre, V
Lasue, J
Meslin, PY
Leveille, RJ
Barraclough, L
Beck, P
Bender, SC
Berger, G
Bridges, JC
Bridges, NT
Dromart, G
Dyar, MD
Francis, R
Frydenvang, J
Gondet, B
Ehlmann, BL
Herkenhoff, KE
Johnson, JR
Langevin, Y
Madsen, MB
Melikechi, N
Lacour, JL
Le Mouelic, S
Lewin, E
Newsom, HE
Ollila, AM
Pinet, P
Schroder, S
Sirven, JB
Tokar, RL
Toplis, MJ
d'Uston, C
Vaniman, DT
Vasavada, AR
AF Maurice, S.
Clegg, S. M.
Wiens, R. C.
Gasnault, O.
Rapin, W.
Forni, O.
Cousin, A.
Sautter, V.
Mangold, N.
Le Deit, L.
Nachon, M.
Anderson, R. B.
Lanza, N. L.
Fabre, C.
Payre, V.
Lasue, J.
Meslin, P. -Y.
Leveille, R. J.
Barraclough, L.
Beck, P.
Bender, S. C.
Berger, G.
Bridges, J. C.
Bridges, N. T.
Dromart, G.
Dyar, M. D.
Francis, R.
Frydenvang, J.
Gondet, B.
Ehlmann, B. L.
Herkenhoff, K. E.
Johnson, J. R.
Langevin, Y.
Madsen, M. B.
Melikechi, N.
Lacour, J. -L.
Le Mouelic, S.
Lewin, E.
Newsom, H. E.
Ollila, A. M.
Pinet, P.
Schroeder, S.
Sirven, J. -B.
Tokar, R. L.
Toplis, M. J.
d'Uston, C.
Vaniman, D. T.
Vasavada, A. R.
TI ChemCam activities and discoveries during the nominal mission of the
Mars Science Laboratory in Gale crater, Mars
SO JOURNAL OF ANALYTICAL ATOMIC SPECTROMETRY
LA English
DT Article
ID INDUCED BREAKDOWN SPECTROSCOPY; CURIOSITY ROVER; OMEGA/MARS EXPRESS;
SPACE EXPLORATION; INSTRUMENT SUITE; YELLOWKNIFE BAY; CHEMISTRY; ORIGIN;
ROCKS; TARGETS
AB At Gale crater, Mars, ChemCam acquired its first laser-induced breakdown spectroscopy (LIBS) target on Sol 13 of the landed portion of the mission (a Sol is a Mars day). Up to Sol 800, more than 188 000 LIBS spectra were acquired on more than 5800 points distributed over about 650 individual targets. We present a comprehensive review of ChemCam scientific accomplishments during that period, together with a focus on the lessons learned from the first use of LIBS in space. For data processing, we describe new tools that had to be developed to account for the uniqueness of Mars data. With regard to chemistry, we present a summary of the composition range measured on Mars for major-element oxides (SiO2, TiO2, Al2O3, FeOT, MgO, CaO, Na2O, K2O) based on various multivariate models, with associated precisions. ChemCam also observed H, and the non-metallic elements C, O, P, and S, which are usually difficult to quantify with LIBS. F and Cl are observed through their molecular lines. We discuss the most relevant LIBS lines for detection of minor and trace elements (Li, Rb, Sr, Ba, Cr, Mn, Ni, and Zn). These results were obtained thanks to comprehensive ground reference datasets, which are set to mimic the expected mineralogy and chemistry on Mars. With regard to the first use of LIBS in space, we analyze and quantify, often for the first time, each of the advantages of using stand-off LIBS in space: no sample preparation, analysis within its petrological context, dust removal, sub-millimeter scale investigation, multi-point analysis, the ability to carry out statistical surveys and whole-rock analyses, and rapid data acquisition. We conclude with a discussion of ChemCam performance to survey the geochemistry of Mars, and its valuable support of decisions about selecting where and whether to make observations with more time and resource-intensive tools in the rover's instrument suite. In the end, we present a bird's-eye view of the many scientific results: discovery of felsic Noachian crust, first observation of hydrated soil, discovery of manganese-rich coatings and fracture fills indicating strong oxidation potential in Mars' early atmosphere, characterization of soils by grain size, and wide scale mapping of sedimentary strata, conglomerates, and diagenetic materials.
C1 [Maurice, S.; Gasnault, O.; Rapin, W.; Forni, O.; Cousin, A.; Lasue, J.; Meslin, P. -Y.; Berger, G.; Schroeder, S.; Toplis, M. J.; d'Uston, C.] Univ Toulouse 3, CNRS, IRAP, Obs Midi Pyrenees, 9 Av Colonel Roche, F-31400 Toulouse, France.
[Clegg, S. M.; Wiens, R. C.; Lanza, N. L.; Barraclough, L.; Frydenvang, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Sautter, V.; Anderson, R. B.] Museum Natl Hist Nat, IMPMC, F-75231 Paris, France.
[Mangold, N.; Le Deit, L.; Nachon, M.; Le Mouelic, S.] LPG Nantes, UMR CNRS 6112, Lab Planetol & Geodynam, Nantes, France.
[Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Fabre, C.; Payre, V.] Univ Lorraine, GeoRessources, Vandoeuvre Les Nancy, France.
[Leveille, R. J.] Canadian Space Agcy, St Hubert, PQ, Canada.
[Leveille, R. J.] McGill Univ, Dept Nat Resource Sci, Montreal, PQ, Canada.
[Beck, P.] Univ Grenoble Alpes, Inst Planetol & Astrophys Grenoble, Grenoble, France.
[Bender, S. C.; Tokar, R. L.; Vaniman, D. T.] Planetary Sci Inst, Tucson, AZ USA.
[Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England.
[Bridges, N. T.; Johnson, J. R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Dromart, G.] Univ Lyon, ENS Lyon, Lab Geol Lyon, Lyon, France.
[Dyar, M. D.] Mt Holyoke Coll, Dept Astron, South Hadley, MA USA.
[Francis, R.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON, Canada.
[Francis, R.; Ehlmann, B. L.; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gondet, B.; Langevin, Y.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
[Melikechi, N.] Delaware State Univ, Opt Sci Ctr Appl Res, Dover, DE USA.
[Lacour, J. -L.; Sirven, J. -B.] Commissariat Energie Atom & Energies Alternat, DEN, Dept Phys Chem, Saclay, France.
[Lewin, E.] Univ Grenoble 1, CNRS, Inst Sci Terre, Grenoble, France.
[Newsom, H. E.; Ollila, A. M.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Newsom, H. E.; Ollila, A. M.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
RP Maurice, S (reprint author), Univ Toulouse 3, CNRS, IRAP, Obs Midi Pyrenees, 9 Av Colonel Roche, F-31400 Toulouse, France.
EM maurice@cesr.fr
RI Frydenvang, Jens/D-4781-2013; Beck, Pierre/F-3149-2011; Sirven,
Jean-Baptiste/H-5782-2013; LEWIN, Eric/F-1451-2017;
OI Frydenvang, Jens/0000-0001-9294-1227; Sirven,
Jean-Baptiste/0000-0002-5523-6809; Clegg, Sam/0000-0002-0338-0948
FU France by the French Space Agency (CNES); Centre National de la
Recherche Scientifique (CNRS); NASA's Mars Program Office
FX This work was supported in France by the French Space Agency (CNES), the
Centre National de la Recherche Scientifique (CNRS), and many institutes
and universities across the country. Collaboration with colleagues in
the US was funded by NASA's Mars Program Office.
NR 107
TC 7
Z9 7
U1 14
U2 36
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 0267-9477
EI 1364-5544
J9 J ANAL ATOM SPECTROM
JI J. Anal. At. Spectrom.
PY 2016
VL 31
IS 4
BP 863
EP 889
DI 10.1039/c5ja00417a
PG 27
WC Chemistry, Analytical; Spectroscopy
SC Chemistry; Spectroscopy
GA DI4LC
UT WOS:000373470400003
ER
PT J
AU Li, WQ
Beard, BL
Li, SL
AF Li, Weiqiang
Beard, Brian L.
Li, Shilei
TI Precise measurement of stable potassium isotope ratios using a single
focusing collision cell multi-collector ICP-MS
SO JOURNAL OF ANALYTICAL ATOMIC SPECTROMETRY
LA English
DT Article
ID PLASMA-MASS-SPECTROMETRY; AUSTRALASIAN TEKTITES; CONTACT REGION; PLANTS;
FRACTIONATION; MOVEMENT; CALCIUM; ZINC; LI
AB High precision potassium isotope ratio measurements were made using a collision-cell equipped single focusing Multi-Collector Inductively Coupled Plasma Mass Spectrometer (MC-ICP-MS). Interferences on K-41 from (ArH+)-Ar-40 were largely suppressed through collision with He gas atoms, and reaction with H-2 or D-2 gas molecules in the collision cell under optimum collision gas flow conditions. Using H-2 or D-2 as the collision gas, we distinguish charged argon-deuterium molecules (ArD+) generated in the collision cell from argon hydride (ArH+) generated in the plasma or in the interface region (referred to as "plasma-related AH(+)" hereafter), and demonstrate, for the first time, that both plasma-related and collision cell-generated ArH+ are important sources of ArH+ that interfere with K-41(+) in collision-cell ICP-MS instruments that use H-2 as a collision gas. The use of D-2 instead of H-2 as a reactive gas in the collision cell resulted in better overall performance in K isotope ratio measurements. By combining these mass spectrometry methods with chemical purification of K by ion exchange chromatography, we achieved an internal precision of <+/- 0.07 parts per thousand (2 standard error) and an external reproducibility of <+/- 0.21 parts per thousand (2 standard deviation, or 95% confidence) in the K-41/K-39 ratio measurement for geological and biological samples. With the improved precision, it is possible to distinguish a similar to 1.3 parts per thousand variation in K isotope compositions (K-41/K-39 ratios) among seawater, igneous rocks, and biological samples. The K isotope system is likely to be beneficial in providing a better understanding of potassium cycling during continental weathering and the uptake of nutrients by plants.
C1 [Li, Weiqiang] Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210046, Jiangsu, Peoples R China.
[Li, Weiqiang] Nanjing Univ, Lunar & Planetary Sci Inst, Nanjing 210046, Jiangsu, Peoples R China.
[Beard, Brian L.] Univ Wisconsin, Dept Geosci, 1215W Dayton St, Madison, WI 53706 USA.
[Beard, Brian L.] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI USA.
[Li, Shilei] Nanjing Univ, Sch Earth Sci & Engn, MOE Key Lab Surficial Geochem, Nanjing 210046, Jiangsu, Peoples R China.
RP Li, WQ (reprint author), Nanjing Univ, Sch Earth Sci & Engn, State Key Lab Mineral Deposits Res, Nanjing 210046, Jiangsu, Peoples R China.; Li, WQ (reprint author), Nanjing Univ, Lunar & Planetary Sci Inst, Nanjing 210046, Jiangsu, Peoples R China.
EM liweiqiang@nju.edu.cn
RI Li, Weiqiang/D-2975-2011
OI Li, Weiqiang/0000-0003-2648-7630
FU "1000-talent Program" of China; NASA Astrobiology Institute
FX This study benefited from constructive comments from two anonymous
reviewers. This study was supported by "1000-talent Program" of China to
W.L. This study was also supported by the NASA Astrobiology Institute.
This is publication No. 1 from Lunar and Planetary Science Institute,
Nanjing University.
NR 28
TC 4
Z9 4
U1 9
U2 17
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 0267-9477
EI 1364-5544
J9 J ANAL ATOM SPECTROM
JI J. Anal. At. Spectrom.
PY 2016
VL 31
IS 4
BP 1023
EP 1029
DI 10.1039/c5ja00487j
PG 7
WC Chemistry, Analytical; Spectroscopy
SC Chemistry; Spectroscopy
GA DI4LC
UT WOS:000373470400018
ER
PT J
AU Zhang, X
Gurney, KR
Rayner, P
Baker, D
Liu, YP
AF Zhang, Xia
Gurney, Kevin R.
Rayner, Peter
Baker, David
Liu, Yu-ping
TI Sensitivity of simulated CO2 concentration to sub-annual variations in
fossil fuel CO2 emissions
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID ATMOSPHERIC CARBON-DIOXIDE; TRANSPORT MODELS; INVERSIONS; UNCERTAINTIES;
EXCHANGE; RECORD; BUDGET; SINKS
AB Recent advances in fossil fuel CO2 (FFCO2) emission inventories enable sensitivity tests of simulated atmospheric CO2 concentrations to sub-annual variations in FFCO2 emissions and what this implies for the interpretation of observed CO2. Six experiments are conducted to investigate the potential impact of three cycles of FFCO2 emission variability (diurnal, weekly and monthly) using a global tracer transport model. Results show an annual FFCO2 rectification varying from -1.35 to +0.13 ppm from the combination of all three cycles. This rectification is driven by a large negative diurnal FFCO2 rectification due to the covariation of diurnal FFCO2 emissions and diurnal vertical mixing, as well as a smaller positive seasonal FFCO2 rectification driven by the covariation of monthly FFCO2 emissions and monthly atmospheric transport. The diurnal FFCO2 emissions are responsible for a diurnal FFCO2 concentration amplitude of up to 9.12 ppm at the grid cell scale. Similarly, the monthly FFCO2 emissions are responsible for a simulated seasonal Cv amplitude of up to 6.11 ppm at the grid cell scale. The impact of the diurnal FFCO2 emissions, when only sampled in the local afternoon, is also important, causing an increase of +1.13 ppmv at the grid cell scale. The simulated CO2 concentration impacts from the diurnally and seasonally varying FFCO2 emissions are centered over large source regions in the Northern Hemisphere, extending to downwind regions. This study demonstrates the influence of sub-annual variations in FFCO2 emissions on simulated CO2 concentration and suggests that inversion studies must take account of these variations in the affected regions.
C1 [Zhang, Xia; Gurney, Kevin R.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA.
[Zhang, Xia] San Diego State Univ, Coll Sci, San Diego, CA 92182 USA.
[Rayner, Peter] Univ Melbourne, Earth Sci, Melbourne, Vic, Australia.
[Baker, David] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Liu, Yu-ping] Sci Syst & Applicat Inc, Lab Atmosphere, NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD USA.
RP Zhang, X (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ USA.; Zhang, X (reprint author), San Diego State Univ, Coll Sci, San Diego, CA 92182 USA.
EM tyouxia@gmail.com
FU National Science Foundation CAREER [0846358]; NASA ROSES grant
[NNX11AH86G]; Australian professorial fellowship [DP1096309]
FX This work was supported by the National Science Foundation CAREER award
0846358 and NASA ROSES grant NNX11AH86G. P. Rayner is supported by an
Australian professorial fellowship (DP1096309).
NR 36
TC 0
Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 1907
EP 1918
DI 10.5194/acp-16-1907-2016
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500004
ER
PT J
AU Park, SS
Kim, J
Lee, H
Torres, O
Lee, KM
Lee, SD
AF Park, Sang Seo
Kim, Jhoon
Lee, Hanlim
Torres, Omar
Lee, Kwang-Mog
Lee, Sang Deok
TI Utilization of O-4 slant column density to derive aerosol layer height
from a space-borne UV-visible hyperspectral sensor: sensitivity and case
study
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID ABSORPTION SPECTROSCOPY DOAS; OZONE MONITORING INSTRUMENT; MAX-DOAS;
OPTICAL-PROPERTIES; UNITED-STATES; AIR-QUALITY; ANTHROPOGENIC SULFATE;
VERTICAL-DISTRIBUTION; ATMOSPHERIC AEROSOLS; RETRIEVAL ALGORITHM
AB The sensitivities of oxygen-dimer (O-4) slant column densities (SCDs) to changes in aerosol layer height are investigated using the simulated radiances by a radiative transfer model, the linearized pseudo-spherical vector discrete ordinate radiative transfer (VLIDORT), and the differential optical absorption spectroscopy (DOAS) technique. The sensitivities of the O4 index (O4I), which is defined as dividing O-4 SCD by 10(40) molecules(2) cm(-5), to aerosol types and optical properties are also evaluated and compared. Among the O-4 absorption bands at 340, 360, 380, and 477 nm, the O-4 absorption band at 477 nm is found to be the most suitable to retrieve the aerosol effective height. However, the O4I at 477 nm is significantly influenced not only by the aerosol layer effective height but also by aerosol vertical profiles, optical properties including single scattering albedo (SSA), aerosol optical depth (AOD), particle size, and surface albedo. Overall, the error of the retrieved aerosol effective height is estimated to be 1276, 846, and 739m for dust, non-absorbing, and absorbing aerosol, respectively, assuming knowledge on the aerosol vertical distribution shape. Using radiance data from the Ozone Monitoring Instrument (OMI), a new algorithm is developed to derive the aerosol effective height over East Asia after the determination of the aerosol type and AOD from the MODerate resolution Imaging Spectroradiometer (MODIS). About 80% of retrieved aerosol effective heights are within the error range of 1 km compared to those obtained from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) measurements on thick aerosol layer cases.
C1 [Park, Sang Seo; Kim, Jhoon; Lee, Hanlim] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Lee, Hanlim] Pukyong Natl Univ, Dept Spatial Informat Engn, Busan 608737, South Korea.
[Torres, Omar] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lee, Kwang-Mog] Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu, South Korea.
[Lee, Sang Deok] Minist Environm, Natl Inst Environm Res, Inchon, South Korea.
[Park, Sang Seo] Kyushu Univ, Appl Mech Res Inst, Fukuoka 812, Japan.
RP Kim, J (reprint author), Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
EM jkim2@yonsei.ac.kr
RI Kyushu, RIAM/F-4018-2015
FU KEITI, South Korea [2012000160002]; Brain Korea PLUS program
FX This work was supported by the Eco Innovation Program of KEITI (grant
no. 2012000160002), South Korea, and by the Brain Korea PLUS program.
NR 93
TC 2
Z9 2
U1 2
U2 8
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 1987
EP 2006
DI 10.5194/acp-16-1987-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500009
ER
PT J
AU Kipling, Z
Stier, P
Johnson, CE
Mann, GW
Bellouin, N
Bauer, SE
Bergman, T
Chin, M
Diehl, T
Ghan, SJ
Iversen, T
Kirkevag, A
Kokkola, H
Liu, XH
Luo, G
van Noije, T
Pringle, KJ
von Salzen, K
Schulz, M
Seland, O
Skeie, RB
Takemura, T
Tsigaridis, K
Zhang, K
AF Kipling, Zak
Stier, Philip
Johnson, Colin E.
Mann, Graham W.
Bellouin, Nicolas
Bauer, Susanne E.
Bergman, Tommi
Chin, Mian
Diehl, Thomas
Ghan, Steven J.
Iversen, Trond
Kirkevag, Alf
Kokkola, Harri
Liu, Xiaohong
Luo, Gan
van Noije, Twan
Pringle, Kirsty J.
von Salzen, Knut
Schulz, Michael
Seland, Oyvind
Skeie, Ragnhild B.
Takemura, Toshihiko
Tsigaridis, Kostas
Zhang, Kai
TI What controls the vertical distribution of aerosol? Relationships
between process sensitivity in HadGEM3-UKCA and inter-model variation
from AeroCom Phase II
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID LOG-NORMAL APPROXIMATION; CHEMISTRY-CLIMATE MODEL; BLACK CARBON;
AIRCRAFT OBSERVATIONS; SIZE DISTRIBUTIONS; ABSORBING AEROSOLS; SULFUR
EMISSIONS; UNIFIED MODEL; MINERAL DUST; GLOMAP-MODE
AB The vertical profile of aerosol is important for its radiative effects, but weakly constrained by observations on the global scale, and highly variable among different models. To investigate the controlling factors in one particular model, we investigate the effects of individual processes in HadGEM3-UKCA and compare the resulting diversity of aerosol vertical profiles with the inter-model diversity from the AeroCom Phase II control experiment.
In this way we show that (in this model at least) the vertical profile is controlled by a relatively small number of processes, although these vary among aerosol components and particle sizes. We also show that sufficiently coarse variations in these processes can produce a similar diversity to that among different models in terms of the global-mean profile and, to a lesser extent, the zonal-mean vertical position. However, there are features of certain models' profiles that cannot be reproduced, suggesting the influence of further structural differences between models.
In HadGEM3-UKCA, convective transport is found to be very important in controlling the vertical profile of all aerosol components by mass. In-cloud scavenging is very important for all except mineral dust. Growth by condensation is important for sulfate and carbonaceous aerosol (along with aqueous oxidation for the former and ageing by soluble material for the latter). The vertical extent of biomass-burning emissions into the free troposphere is also important for the profile of carbonaceous aerosol. Boundary-layer mixing plays a dominant role for sea salt and mineral dust, which are emitted only from the surface. Dry deposition and below-cloud scavenging are important for the profile of mineral dust only.
In this model, the microphysical processes of nucleation, condensation and coagulation dominate the vertical profile of the smallest particles by number (e.g. total CN > 3 nm), while the profiles of larger particles (e.g. CN > 100 nm) are controlled by the same processes as the component mass profiles, plus the size distribution of primary emissions.
We also show that the processes that affect the AOD-normalised radiative forcing in the model are predominantly those that affect the vertical mass distribution, in particular convective transport, in-cloud scavenging, aqueous oxidation, ageing and the vertical extent of biomass-burning emissions.
C1 [Kipling, Zak; Stier, Philip] Univ Oxford, Dept Phys, Oxford, England.
[Johnson, Colin E.] Met Off Hadley Ctr, Exeter, Devon, England.
[Mann, Graham W.] Univ Leeds, Natl Ctr Atmospher Sci, Leeds, W Yorkshire, England.
[Mann, Graham W.; Pringle, Kirsty J.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Bellouin, Nicolas] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Bauer, Susanne E.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Bauer, Susanne E.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bergman, Tommi; Kokkola, Harri] Atmospher Res Ctr Eastern Finland, Finnish Meteorol Inst, Kuopio, Finland.
[Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Diehl, Thomas] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, Climate Risk Management Unit, Ispra, Italy.
[Ghan, Steven J.; Zhang, Kai] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Iversen, Trond; Kirkevag, Alf; Schulz, Michael; Seland, Oyvind] Norwegian Meteorol Inst, Oslo, Norway.
[Iversen, Trond] Univ Oslo, Dept Geosci, Oslo, Norway.
[Liu, Xiaohong] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Luo, Gan] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA.
[van Noije, Twan] Royal Netherlands Meteorol Inst, POB 201, NL-3730 AE De Bilt, Netherlands.
[von Salzen, Knut] Environm Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Skeie, Ragnhild B.] Ctr Int Climate & Environm Res Oslo, Oslo, Norway.
[Takemura, Toshihiko] Kyushu Univ, Appl Mech Res Inst, Fukuoka 812, Japan.
[Zhang, Kai] Max Planck Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany.
RP Kipling, Z (reprint author), Univ Oxford, Dept Phys, Oxford, England.
EM zak.kipling@physics.ox.ac.uk
RI Ghan, Steven/H-4301-2011; Takemura, Toshihiko/C-2822-2009; Kyushu,
RIAM/F-4018-2015; Stier, Philip/B-2258-2008; Zhang, Kai/F-8415-2010;
Skeie, Ragnhild/K-1173-2015; Bergman, Tommi/C-2445-2009; Chin,
Mian/J-8354-2012; Liu, Xiaohong/E-9304-2011; Kokkola, Harri/J-5993-2014;
OI Ghan, Steven/0000-0001-8355-8699; Takemura,
Toshihiko/0000-0002-2859-6067; Stier, Philip/0000-0002-1191-0128; Zhang,
Kai/0000-0003-0457-6368; Skeie, Ragnhild/0000-0003-1246-4446; Bergman,
Tommi/0000-0002-6133-2231; Liu, Xiaohong/0000-0002-3994-5955; Bellouin,
Nicolas/0000-0003-2109-9559
FU Natural Environment Research Council [NE/J022624/1]; Met Office;
European Research Council under the European Union/ERC [FP7-280025];
Natural Environment Research Council (NERC) through the National Centre
for Atmospheric Science (NCAS); Academy of Finland Centre of Excellence
[272041]; US Department of Energy Office of Science Decadal and Regional
Climate Prediction using Earth System Models (EaSM) programme; DOE
[DE-AC06-76RLO 1830]; Research Council of Norway through the EarthClim
[207711/E10]; EVA [229771]; NOTUR/NorStore projects, by the Norwegian
Space Centre through PM-VRAE; EU; Canadian Foundation for Climate and
Atmospheric Sciences (CFCAS); Environment Canada; Research Council of
Norway; supercomputer system of the National Institute for Environmental
Studies, Japan; Ministry of the Environment, Japan [S-12-3]; JSPS
KAKENHI [15H01728, 15K12190]; NASA-MAP (NASA) [NNX09AK32G]; Max Planck
Society
FX This work was supported by the Natural Environment Research Council
project GASSP (grant number NE/J022624/1) and the Met Office. P. Stier
would like to acknowledge funding from the European Research Council
under the European Union's Seventh Framework Programme
(FP7/2007-2013)/ERC grant agreement no. FP7-280025. G. W. Mann was
supported by the Natural Environment Research Council (NERC) through the
National Centre for Atmospheric Science (NCAS). T. Bergman and H.
Kokkola were supported by the Academy of Finland Centre of Excellence
(project no. 272041). S. Ghan and X. Liu were supported by the US
Department of Energy Office of Science Decadal and Regional Climate
Prediction using Earth System Models (EaSM) programme. The Pacific
Northwest National Laboratory (PNNL) is operated for the DOE by Battelle
Memorial Institute under contract DE-AC06-76RLO 1830. A. Kirkevag, T.
Iversen and O. Seland (CAM4-Oslo) were supported by the Research Council
of Norway through the EarthClim (207711/E10), EVA (229771) and
NOTUR/NorStore projects, by the Norwegian Space Centre through PM-VRAE,
and through the EU projects PEGASOS and ACCESS. K. von Salzen was
supported by the Canadian Foundation for Climate and Atmospheric
Sciences (CFCAS) and Environment Canada. R. B. Skeie (OsloCTM2) was
supported by the Research Council of Norway, through the grants SLAC,
AEROCOM-P3 and ClimSense. T. Takemura was supported by the supercomputer
system of the National Institute for Environmental Studies, Japan, the
Environment Research and Technology Development Fund (S-12-3) of the
Ministry of the Environment, Japan, and JSPS KAKENHI (grant numbers
15H01728 and 15K12190). K. Tsigaridis and S. E. Bauer were supported by
NASA-MAP (NASA award number: NNX09AK32G). Resources supporting this work
were provided by the NASA High-End Computing (HEC) Program through the
NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center. K. Zhang was supported by funding from the Max Planck Society.
Simulations with ECHAM5-HAM2 were performed at the German Climate
Computing Center (Deutsches Klimarechenzentrum GmbH, DKRZ).
NR 90
TC 4
Z9 4
U1 2
U2 14
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 2221
EP 2241
DI 10.5194/acp-16-2221-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500023
ER
PT J
AU Hammer, MS
Martin, RV
van Donkelaar, A
Buchard, V
Torres, O
Ridley, DA
Spurr, RJD
AF Hammer, Melanie S.
Martin, Randall V.
van Donkelaar, Aaron
Buchard, Virginie
Torres, Omar
Ridley, David A.
Spurr, Robert J. D.
TI Interpreting the ultraviolet aerosol index observed with the OMI
satellite instrument to understand absorption by organic aerosols:
implications for atmospheric oxidation and direct radiative effects
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID COMPLEX REFRACTIVE-INDEXES; SINGLE SCATTERING ALBEDO; BROWN CARBON
AEROSOL; LIGHT-ABSORPTION; BLACK CARBON; SPECTRAL DEPENDENCE; ANGSTROM
EXPONENT; TROPOSPHERIC CHEMISTRY; GLOBAL DISTRIBUTION; PARTICULATE
MATTER
AB Satellite observations of the ultraviolet aerosol index (UVAI) are sensitive to absorption of solar radiation by aerosols; this absorption affects photolysis frequencies and radiative forcing. We develop a global simulation of the UVAI using the 3-D chemical transport model GEOS-Chem coupled with the Vector Linearized Discrete Ordinate Radiative Transfer model (VLIDORT). The simulation is applied to interpret UVAI observations from the Ozone Monitoring Instrument (OMI) for the year 2007. Simulated and observed values are highly consistent in regions where mineral dust dominates the UVAI, but a large negative bias (0-.32 to -0.97) exists between simulated and observed values in biomass burning regions. We determine effective optical properties for absorbing organic aerosol, known as brown carbon (BrC), and implement them into GEOS-Chem to better represent observed UVAI values over biomass burning regions. The inclusion of absorbing BrC decreases the mean bias between simulated and OMI UVAI values from -0.57 to -0.09 over West Africa in January, from -0.32 to +0.0002 over South Asia in April, from -0.97 to -0.22 over southern Africa in July, and from -0.50 to +0.33 over South America in September. The spectral dependence of absorption after including BrC in the model is broadly consistent with reported observations for biomass burning aerosol, with absorbing ngstrm exponent (AAE) values ranging from 2.9 in the ultraviolet (UV) to 1.3 across the UV-Near IR spectrum. We assess the effect of the additional UV absorption by BrC on atmospheric photochemistry by examining tropospheric hydroxyl radical (OH) concentrations in GEOS-Chem. The inclusion of BrC decreases OH by up to 30% over South America in September, up to 20% over southern Africa in July, and up to 15% over other biomass burning regions. Global annual mean OH concentrations in GEOS-Chem decrease due to the presence of absorbing BrC, increasing the methyl chloroform lifetime from 5.62 to 5.68 years, thus reducing the bias against observed values. We calculate the direct radiative effect (DRE) of BrC using GEOS-Chem coupled with the radiative transfer model RRTMG (GC-RT). Treating organic aerosol as containing more strongly absorbing BrC changes the global annual mean all-sky top of atmosphere (TOA) DRE by +0.03 Wm(-2) and all-sky surface DRE by -0.08 Wm(-2). Regional changes of up to +0.3 Wm(-2) at TOA and down to -1.5 W m(-2) at the surface are found over major biomass burning regions.
C1 [Hammer, Melanie S.; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Buchard, Virginie; Torres, Omar] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Buchard, Virginie] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Ridley, David A.] MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Spurr, Robert J. D.] RT Solut Inc, 9 Channing St, Cambridge, MA USA.
RP Hammer, MS (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
EM melanie.hammer@dal.ca
RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
FU Natural Science and Engineering Research Council of Canada
FX This work was supported by the Natural Science and Engineering Research
Council of Canada. Computational facilities were provided in part by the
Atlantic Computational Excellence Network consortium of Compute Canada.
We thank Farhan Khan for assistance during the early stages of this
work.
NR 87
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Z9 4
U1 3
U2 10
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 2507
EP 2523
DI 10.5194/acp-16-2507-2016
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500040
ER
PT J
AU Pusede, SE
Duffey, KC
Shusterman, AA
Saleh, A
Laughner, JL
Wooldridge, PJ
Zhang, Q
Parworth, CL
Kim, H
Capps, SL
Valin, LC
Cappa, CD
Fried, A
Walega, J
Nowak, JB
Weinheimer, AJ
Hoff, RM
Berkoff, TA
Beyersdorf, AJ
Olson, J
Crawford, JH
Cohen, RC
AF Pusede, S. E.
Duffey, K. C.
Shusterman, A. A.
Saleh, A.
Laughner, J. L.
Wooldridge, P. J.
Zhang, Q.
Parworth, C. L.
Kim, H.
Capps, S. L.
Valin, L. C.
Cappa, C. D.
Fried, A.
Walega, J.
Nowak, J. B.
Weinheimer, A. J.
Hoff, R. M.
Berkoff, T. A.
Beyersdorf, A. J.
Olson, J.
Crawford, J. H.
Cohen, R. C.
TI On the effectiveness of nitrogen oxide reductions as a control over
ammonium nitrate aerosol
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID SAN-JOAQUIN-VALLEY; SECONDARY ORGANIC AEROSOL; THERMODYNAMIC-EQUILIBRIUM
MODEL; FLUORESCENCE TD-LIF; UNITED-STATES; CENTRAL CALIFORNIA; DRY
DEPOSITION; PARTICULATE NITRATE; PEROXY NITRATES; AIR-QUALITY
AB Nitrogen oxides (NOx) have fallen steadily across the US over the last 15 years. At the same time, NOx concentrations decrease on weekends relative to weekdays, largely without co-occurring changes in other gas-phase emissions, due to patterns of diesel truck activities. These trends taken together provide two independent constraints on the role of NO x in the nonlinear chemistry of atmospheric oxidation. In this context, we interpret interannual trends in wintertime ammonium nitrate (NH4NO3) in the San Joaquin Valley of California, a location with the worst aerosol pollution in the US and where a large portion of aerosol mass is NH4NO3. Here, we show that NO x reductions have simultaneously decreased nighttime and increased daytime NH4NO3 production over the last decade. We find a substantial decrease in NH4NO3 since 2000 and conclude that this decrease is due to reduced nitrate radical-initiated production at night in residual layers that are decoupled from fresh emissions at the surface. Further reductions in NOx are imminent in California, and nationwide, and we make a quantitative prediction of the response of NH4NO3. We show that the combination of rapid chemical production and efficient NH4NO3 loss via deposition of gas-phase nitric acid implies that high aerosol days in cities in the San Joaquin Valley air basin are responsive to local changes in NOx within those individual cities. Our calculations indicate that large decreases in NOx in the future will not only lower wintertime NH4NO3 concentrations but also cause a transition in the dominant NH4NO3 source from nighttime to daytime chemistry.
C1 [Pusede, S. E.; Duffey, K. C.; Shusterman, A. A.; Saleh, A.; Laughner, J. L.; Wooldridge, P. J.; Cohen, R. C.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Zhang, Q.; Parworth, C. L.] Univ Calif Davis, Dept Environm Toxicol, Davis, CA 95616 USA.
[Kim, H.] Korea Inst Sci & Technol, Ctr Environm Hlth & Welf Res, Seoul, South Korea.
[Capps, S. L.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Valin, L. C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Cappa, C. D.] Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA.
[Walega, J.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Nowak, J. B.] Aerodyne Res Inc, Billerica, MA 01821 USA.
[Weinheimer, A. J.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Hoff, R. M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Berkoff, T. A.; Beyersdorf, A. J.; Olson, J.; Crawford, J. H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Cohen, R. C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Pusede, S. E.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
RP Cohen, RC (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.; Cohen, RC (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
EM rccohen@berkeley.edu
RI Cohen, Ronald/A-8842-2011; Capps, Shannon/E-5602-2017;
OI Cohen, Ronald/0000-0001-6617-7691; Capps, Shannon/0000-0002-6872-6604;
Nowak, John/0000-0002-5697-9807
FU NASA [NNX10AR36G]; California Air Resources Board [14-307]
FX This work was funded by NASA under grant NNX10AR36G. Q. Zhang and C. D.
Cappa were also supported by the California Air Resources Board
(contract no. 14-307). We acknowledge use of publicly available data
maintained by the US EPA, California Air Resources Board, and California
Irrigation Management Information System. We thank John Barrick for the
jNO2 and RH (PDS) data, Glenn Diskin for the
H2O(v) (DLH) data, Luke Ziemba and Lee Thornhill
for the f (RH) and UHSAS data, and Donald Blake for the speciated
organic compound data. We thank Melinda Beaver for assistance
interpreting the long-term ozone data. We thank Steve S. Brown for his
feedback during the review process. This analysis would not have been
possible without the work of the pilots, crew, and engineers of the NASA
P-3B.
NR 99
TC 3
Z9 3
U1 12
U2 18
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 2575
EP 2596
DI 10.5194/acp-16-2575-2016
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500044
ER
PT J
AU Wolfe, GM
Kaiser, J
Hanisco, TF
Keutsch, FN
de Gouw, JA
Gilman, JB
Graus, M
Hatch, CD
Holloway, J
Horowitz, LW
Lee, BH
Lerner, BM
Lopez-Hilifiker, F
Mao, J
Marvin, MR
Peischl, J
Pollack, IB
Roberts, JM
Ryerson, TB
Thornton, JA
Veres, PR
Warneke, C
AF Wolfe, G. M.
Kaiser, J.
Hanisco, T. F.
Keutsch, F. N.
de Gouw, J. A.
Gilman, J. B.
Graus, M.
Hatch, C. D.
Holloway, J.
Horowitz, L. W.
Lee, B. H.
Lerner, B. M.
Lopez-Hilifiker, F.
Mao, J.
Marvin, M. R.
Peischl, J.
Pollack, I. B.
Roberts, J. M.
Ryerson, T. B.
Thornton, J. A.
Veres, P. R.
Warneke, C.
TI Formaldehyde production from isoprene oxidation across NOx regimes
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID METHYL VINYL KETONE; OZONE MONITORING INSTRUMENT; ORGANIC-COMPOUND
EMISSIONS; AIRBORNE FLUX MEASUREMENTS; ATMOSPHERIC CHEMISTRY;
UNITED-STATES; RATE CONSTANTS; IMPACT; METHACROLEIN; AEROSOL
AB The chemical link between isoprene and formaldehyde (HCHO) is a strong, nonlinear function of NOx (i. e., NO + NO2). This relationship is a linchpin for top-down isoprene emission inventory verification from orbital HCHO column observations. It is also a benchmark for overall photochemical mechanism performance with regard to VOC oxidation. Using a comprehensive suite of airborne in situ observations over the southeast US, we quantify HCHO production across the urban-rural spectrum. Analysis of isoprene and its major first-generation oxidation products allows us to define both a "prompt" yield of HCHO (molecules of HCHO produced per molecule of freshly emitted isoprene) and the background HCHO mixing ratio (from oxidation of longer-lived hydrocarbons). Over the range of observed NOx values (roughly 0.1-2 ppbv), the prompt yield increases by a factor of 3 (from 0.3 to 0.9 ppbv ppbv(-1)), while background HCHO increases by a factor of 2 (from 1.6 to 3.3 ppbv). We apply the same method to evaluate the performance of both a global chemical transport model (AM3) and a measurement-constrained 0-D steady-state box model. Both models reproduce the NOx dependence of the prompt HCHO yield, illustrating that models with updated isoprene oxidation mechanisms can adequately capture the link between HCHO and recent isoprene emissions. On the other hand, both models underestimate background HCHO mixing ratios, suggesting missing HCHO precursors, inadequate representation of later-generation isoprene degradation and/or underestimated hydroxyl radical concentrations. Detailed process rates from the box model simulation demonstrate a 3-fold increase in HCHO production across the range of observed NOx values, driven by a 100% increase in OH and a 40% increase in branching of organic peroxy radical reactions to produce HCHO.
C1 [Wolfe, G. M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Wolfe, G. M.; Hanisco, T. F.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Kaiser, J.] Univ Wisconsin, Dept Chem, 1101 Univ Ave, Madison, WI 53706 USA.
[Keutsch, F. N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Keutsch, F. N.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[de Gouw, J. A.; Gilman, J. B.; Graus, M.; Holloway, J.; Lerner, B. M.; Peischl, J.; Pollack, I. B.; Veres, P. R.; Warneke, C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[de Gouw, J. A.; Gilman, J. B.; Graus, M.; Holloway, J.; Lerner, B. M.; Peischl, J.; Pollack, I. B.; Roberts, J. M.; Ryerson, T. B.; Veres, P. R.; Warneke, C.] NOAA, Earth Syst Res Lab, Chem Sci Div, Boulder, CO USA.
[Hatch, C. D.] Hendrix Coll, Dept Chem, Conway, AR USA.
[Horowitz, L. W.; Mao, J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Lee, B. H.; Lopez-Hilifiker, F.; Thornton, J. A.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Marvin, M. R.] Univ Maryland, Dept Chem, College Pk, MD 20742 USA.
[Mao, J.] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Graus, M.] Univ Innsbruck, Inst Atmospher & Cryospher Sci, A-6020 Innsbruck, Austria.
[Lopez-Hilifiker, F.] Paul Scherrer Inst, Lab Atmospher Chem, CH-5232 Villigen, Switzerland.
RP Wolfe, GM (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.; Wolfe, GM (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
EM glenn.m.wolfe@nasa.gov
RI Manager, CSD Publications/B-2789-2015; Mao, Jingqiu/F-2511-2010; de
Gouw, Joost/A-9675-2008; Peischl, Jeff/E-7454-2010; Veres,
Patrick/E-7441-2010; Roberts, James/A-1082-2009; Wolfe,
Glenn/D-5289-2011; Gilman, Jessica/E-7751-2010; Pollack,
Ilana/F-9875-2012; Thornton, Joel/C-1142-2009
OI Mao, Jingqiu/0000-0002-4774-9751; de Gouw, Joost/0000-0002-0385-1826;
Peischl, Jeff/0000-0002-9320-7101; Veres, Patrick/0000-0001-7539-353X;
Roberts, James/0000-0002-8485-8172; Gilman, Jessica/0000-0002-7899-9948;
Thornton, Joel/0000-0002-5098-4867
FU US EPA Science to Achieve Results (STAR) program [83540601]; NASA
[NNH10ZDA001N-SEAC4RS]; NASA ACCDAM grant [NNX14AP48G]; NASA ESSF grant
[NNX14AK97H]; Hendrix faculty grant; Hendrix College Odyssey program;
NOAA Climate Program Office [NA13OAR4310071]
FX We are grateful to NOAA AOC and the flight crew of the WP-3D for
enabling a super awesome mission. HCHO measurement efforts were
supported by US EPA Science to Achieve Results (STAR) program grant
83540601 and NASA grant NNH10ZDA001N-SEAC4RS. Analysis was supported by
NASA ACCDAM grant NNX14AP48G. J. Kaiser acknowledges support from NASA
ESSF grant NNX14AK97H. C. D. Hatch was supported by the Hendrix faculty
grant and the Hendrix College Odyssey program. J. Mao and L. W. Horowitz
acknowledge support from NOAA Climate Program Office grant #
NA13OAR4310071. This research has not been subjected to any EPA review
and therefore does not necessarily reflect the views of the agency, and
no official endorsement should be inferred.
NR 80
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U2 41
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 2597
EP 2610
DI 10.5194/acp-16-2597-2016
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500045
ER
PT J
AU Sullivan, SC
Betancourt, RM
Barahona, D
Nenes, A
AF Sullivan, Sylvia C.
Betancourt, Ricardo Morales
Barahona, Donifan
Nenes, Athanasios
TI Understanding cirrus ice crystal number variability for different
heterogeneous ice nucleation spectra
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID MINERAL DUST PARTICLES; ATMOSPHERE MODEL CAM5; CLOUD FORMATION;
EMPIRICAL PARAMETERIZATION; AIRCRAFT MEASUREMENTS; FREEZING NUCLEATION;
MIDLATITUDE CIRRUS; DROPLET NUMBER; CLIMATE MODELS; CONTACT-ANGLE
AB Along with minimizing parameter uncertainty, understanding the cause of temporal and spatial variability of the nucleated ice crystal number, Ni, is key to improving the representation of cirrus clouds in climate models. To this end, sensitivities of Ni to input variables like aerosol number and diameter provide valuable information about nucleation regime and efficiency for a given model formulation. Here we use the adjoint model of the adjoint of a cirrus formation parameterization (Barahona and Nenes, 2009b) to understand Ni variability for various ice-nucleating particle (INP) spectra. Inputs are generated with the Community Atmosphere Model version 5, and simulations are done with a theoretically derived spectrum, an empirical lab-based spectrum and two field-based empirical spectra that differ in the nucleation threshold for black carbon particles and in the active site density for dust. The magnitude and sign of Ni sensitivity to insoluble aerosol number can be directly linked to nucleation regime and efficiency of various INP. The lab-based spectrum calculates much higher INP efficiencies than field-based ones, which reveals a disparity in aerosol surface properties. Ni sensitivity to temperature tends to be low, due to the compensating effects of temperature on INP spectrum parameters; this low temperature sensitivity regime has been experimentally reported before but never deconstructed as done here.
C1 [Sullivan, Sylvia C.; Nenes, Athanasios] Georgia Inst Technol, Dept Chem & Biomol Engn, Atlanta, GA 30332 USA.
[Betancourt, Ricardo Morales] Univ Los Andes, Dept Civil & Environm Engn, Bogota, Colombia.
[Barahona, Donifan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nenes, Athanasios] Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Nenes, Athanasios] Fdn Res & Technol, ICE HT, Patras 26504, Greece.
[Nenes, Athanasios] Natl Observ Athens, IERSD, Palea Penteli 15236, Greece.
RP Nenes, A (reprint author), Georgia Inst Technol, Dept Chem & Biomol Engn, Atlanta, GA 30332 USA.; Nenes, A (reprint author), Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA.; Nenes, A (reprint author), Fdn Res & Technol, ICE HT, Patras 26504, Greece.; Nenes, A (reprint author), Natl Observ Athens, IERSD, Palea Penteli 15236, Greece.
EM athanasios.nenes@gatech.edu
RI Morales Betancourt, Ricardo/A-3827-2016
OI Morales Betancourt, Ricardo/0000-0002-5475-8605
FU DOE EaSM; National Aeronautics and Space Administration Earth and Space
Science Fellowship
FX This work was made possible through support from DOE EaSM. S. C.
Sullivan gratefully acknowledges support from a National Aeronautics and
Space Administration Earth and Space Science Fellowship. We would like
to thank two anonymous reviewers for their thorough and insightful
feedback, in particular for suggestions about measurement-model
comparison. Data in Fig. 2 comes from Andrew Heymsfield's VIPS and Paul
Lawson's TDS measurements aboard the WB57 during MACPEX and from Paul
Lawson's F-FSSP measurements aboard the SPEC Learjet during SPARTICUS.
Thanks also to Heike Kalesse for the use of processed vertical motion
data from SPARTICUS.
NR 79
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Z9 2
U1 7
U2 14
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 4
BP 2611
EP 2629
DI 10.5194/acp-16-2611-2016
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7KC
UT WOS:000372971500046
ER
PT S
AU Bruno, A
Adriani, O
Barbarino, GC
Bazilevskaya, GA
Bellotti, R
Boezio, M
Bogomolov, EA
Bongi, M
Bonvicini, V
Bottai, S
Bravar, U
Cafagna, F
Campana, D
Carbone, R
Carlson, P
Casolino, M
Castellini, G
Christian, EC
De Donato, C
de Nolfo, GA
De Santis, C
De Simone, N
Di Felice, V
Formato, V
Galper, AM
Karelin, AV
Koldashov, SV
Koldobskiy, S
Krutkov, SY
Kvashnin, AN
Lee, M
Leonov, A
Malakhov, V
Marcelli, L
Martucci, M
Mayorov, AG
Menn, W
Merge, M
Mikhailov, VV
Mocchiutti, E
Monaco, A
Mori, N
Munini, R
Osteria, G
Palma, F
Panico, B
Papini, P
Pearce, M
Picozza, P
Ricci, M
Ricciarini, SB
Ryan, JM
Sarkar, R
Scotti, V
Simon, M
Sparvoli, R
Spillantini, P
Stochaj, S
Stozhkov, YI
Vacchi, A
Vannuccini, E
Vasilyev, GI
Voronov, SA
Yurkin, YT
Zampa, G
Zampa, N
Zverev, G
AF Bruno, A.
Adriani, O.
Barbarino, G. C.
Bazilevskaya, G. A.
Bellotti, R.
Boezio, M.
Bogomolov, E. A.
Bongi, M.
Bonvicini, V.
Bottai, S.
Bravar, U.
Cafagna, F.
Campana, D.
Carbone, R.
Carlson, P.
Casolino, M.
Castellini, G.
Christian, E. C.
De Donato, C.
de Nolfo, G. A.
De Santis, C.
De Simone, N.
Di Felice, V.
Formato, V.
Galper, A. M.
Karelin, A. V.
Koldashov, S. V.
Koldobskiy, S.
Krutkov, S. Y.
Kvashnin, A. N.
Lee, M.
Leonov, A.
Malakhov, V.
Marcelli, L.
Martucci, M.
Mayorov, A. G.
Menn, W.
Merge, M.
Mikhailov, V. V.
Mocchiutti, E.
Monaco, A.
Mori, N.
Munini, R.
Osteria, G.
Palma, F.
Panico, B.
Papini, P.
Pearce, M.
Picozza, P.
Ricci, M.
Ricciarini, S. B.
Ryan, J. M.
Sarkar, R.
Scotti, V.
Simon, M.
Sparvoli, R.
Spillantini, P.
Stochaj, S.
Stozhkov, Y. I.
Vacchi, A.
Vannuccini, E.
Vasilyev, G. I.
Voronov, S. A.
Yurkin, Y. T.
Zampa, G.
Zampa, N.
Zverev, G.
GP IOP
TI The May 17, 2012 solar event: back-tracing analysis and flux
reconstruction with PAMELA
SO INTERNATIONAL CONFERENCE ON PARTICLE PHYSICS AND ASTROPHYSICS
(ICPPA-2015), PTS 1-4
SE Journal of Physics Conference Series
LA English
DT Proceedings Paper
CT International Conference on Particle Physics and Astrophysics (ICPPA)
CY OCT 05-10, 2015
CL Moscow, RUSSIA
SP Natl Res Nucl Univ MEPhI, Ctr Fundamental Res & Particle Phys
AB The PAMELA space experiment is providing first direct observations of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth orbit, bridging the low energy measurements by other spacecrafts and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies associated to SEP events. The analysis is supported by an accurate back-tracing simulation based on a realistic description of the Earth's magnetosphere, which is exploited to estimate the SEP energy spectra as a function of the asymptotic direction of arrival with respect to the Interplanetary Magnetic Field (IMF). In this work we report the results for the May 17, 2012 event.
C1 [Bruno, A.; Bellotti, R.; Monaco, A.] Univ Bari Aldo Moro, Dept Phys, I-70126 Bari, Italy.
[Adriani, O.; Bongi, M.; Mori, N.; Spillantini, P.] Univ Florence, Dept Phys & Astron, I-50019 Florence, Italy.
[Adriani, O.; Bongi, M.; Bottai, S.; Mori, N.; Papini, P.; Ricciarini, S. B.; Spillantini, P.; Vannuccini, E.] Ist Nazl Fis Nucl, Sez Florence, I-50019 Florence, Italy.
[Barbarino, G. C.; Scotti, V.] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy.
[Barbarino, G. C.; Campana, D.; Osteria, G.; Panico, B.; Scotti, V.] Ist Nazl Fis Nucl, Sez Naples, I-80126 Naples, Italy.
[Bazilevskaya, G. A.; Kvashnin, A. N.; Stozhkov, Y. I.] Russian Acad Sci, PN Lebedev Phys Inst, RU-119991 Moscow, Russia.
[Bellotti, R.; Cafagna, F.; Monaco, A.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Boezio, M.; Bonvicini, V.; Carbone, R.; Formato, V.; Mocchiutti, E.; Munini, R.; Vacchi, A.; Zampa, G.; Zampa, N.] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy.
[Bogomolov, E. A.; Krutkov, S. Y.; Vasilyev, G. I.] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia.
[Bravar, U.; Lee, M.; Ryan, J. M.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Carlson, P.; Pearce, M.] KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Carlson, P.; Pearce, M.] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Casolino, M.; De Donato, C.; De Santis, C.; De Simone, N.; Di Felice, V.; Marcelli, L.; Merge, M.; Palma, F.; Picozza, P.; Sparvoli, R.] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, I-00133 Rome, Italy.
[Casolino, M.] RIKEN, Adv Sci Inst, Wako, Saitama, Japan.
[Castellini, G.; Ricciarini, S. B.] IFAC, I-50019 Florence, Italy.
[Christian, E. C.; de Nolfo, G. A.] NASA, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Leonov, A.; Malakhov, V.; Mayorov, A. G.; Mikhailov, V. V.; Voronov, S. A.; Yurkin, Y. T.; Zverev, G.] Natl Res Nucl Univ, MEPhI, Moscow Engn Phys Inst, Kashirskoye Highway 31, RU-115409 Moscow, Russia.
[De Donato, C.; De Santis, C.; Marcelli, L.; Martucci, M.; Merge, M.; Palma, F.; Picozza, P.; Sparvoli, R.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy.
[Di Felice, V.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Formato, V.; Munini, R.] Univ Trieste, Dept Phys, I-34147 Trieste, Italy.
[Martucci, M.; Ricci, M.] Ist Nazl Fis Nucl, Lab Nazl Frascati, POB 13, I-00044 Frascati, Italy.
[Menn, W.; Simon, M.] Univ Siegen, Dept Phys, D-57068 Siegen, Germany.
[Sarkar, R.] Indian Ctr Space Phys, 43 Chalantika, Kolkata 700084, W Bengal, India.
[Sarkar, R.] Ist Nazl Fis Nucl, I-34149 Trieste, Italy.
[Stochaj, S.] New Mexico State Univ, Elect & Comp Engn, Las Cruces, NM 88003 USA.
RP Bruno, A (reprint author), Univ Bari Aldo Moro, Dept Phys, I-70126 Bari, Italy.
EM alessandro.bruno@ba.infn.it
RI Mikhailov, Vladimir/B-5368-2014; Karelin, Alexander/O-6576-2016;
Voronov, Sergey/P-9654-2016; Malakhov, Vitaly/Q-6730-2016; Bazilevskaya,
Galina/M-6175-2015; Panico, Beatrice/F-1137-2017; Vacchi,
Andrea/C-1291-2010; Mori, Nicola/D-9459-2016; Mayorov,
Andrey/M-1207-2016; Leonov, Alexey/E-4698-2016; Krutkov,
Sergey/E-7561-2014; Galper, Arkady/M-9610-2015; Koldobskiy,
Sergey/K-6507-2015; Vasilyev, Gennady/E-4843-2014; De Donato,
Cinzia/J-9132-2015; De Santis, Cristian/C-1210-2011; Cafagna,
Francesco/A-9299-2010; marcelli, laura/K-8860-2016; Palma,
Francesco/K-3224-2015; Di Felice, Valeria/L-2989-2016
OI Mikhailov, Vladimir/0000-0003-3851-2901; Voronov,
Sergey/0000-0002-9209-0618; Panico, Beatrice/0000-0003-1063-6961;
Ricciarini, Sergio Bruno/0000-0001-6176-3368; Vacchi,
Andrea/0000-0003-3855-5856; Boezio, Mirko/0000-0002-8015-2981; Mori,
Nicola/0000-0003-2138-3787; Koldobskiy, Sergey/0000-0001-9187-0383; De
Donato, Cinzia/0000-0002-9725-1281; De Santis,
Cristian/0000-0002-7280-2446; Cafagna, Francesco/0000-0002-7450-4784;
marcelli, laura/0000-0002-3180-1228; Palma,
Francesco/0000-0001-7076-8830;
NR 11
TC 0
Z9 0
U1 10
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1742-6588
J9 J PHYS CONF SER
PY 2016
VL 675
AR 032006
DI 10.1088/1742-6596/675/3/032006
PG 5
WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA BE5AH
UT WOS:000372460100072
ER
PT S
AU Topchiev, NP
Galper, AM
Bonvicini, V
Adriani, O
Aptekar, RL
Arkhangelskaja, IV
Arkhangelskiy, AI
Bakaldin, AV
Bergstrom, L
Berti, E
Bigongiari, G
Bobkov, SG
Boezio, M
Bogomolov, EA
Bonechi, L
Bongi, M
Bottai, S
Castellini, G
Cattaneo, PW
Cumani', P
Dalkarov, D
Dedenko, GL
De Donato, C
Dogiel, VA
Finetti, N
Gascon, D
Gorbunov, MS
Gusakov, YV
Hnatyk, BI
Kadilin, VV
Kaplin, VA
Kaplun, AA
Kheymits, MD
Korepanov, VE
Larsson, J
Leonov, AA
Loginov, VA
Longo, F
Maestro, P
Marrocchesi, PS
Martinez, M
Men'shenin, AL
Mikhailov, VV
Mocchiutti, E
Moiseev, AA
Mori, N
Moskalenko, IV
Naumov, PY
Papini, P
Paredes, JM
Pearce, M
Picozza, P
Rappoldi, A
Ricciarini, S
Runtso, MF
Ryde, F
Serdin, OV
Sparvoli, R
Spillantini, P
Stozhkov, YI
Suchkov, SI
Taraskin, AA
Tavani, M
Tiberio, A
Tyurin, EM
Ulanov, MV
Vacchi, A
Vannuccini, E
Vasilyev, GI
Ward, JE
Yurkin, YT
Zampa, N
Zirakashvili, VN
Zverev, VG
AF Topchiev, N. P.
Galper, A. M.
Bonvicini, V.
Adriani, O.
Aptekar, R. L.
Arkhangelskaja, I. V.
Arkhangelskiy, A. I.
Bakaldin, A. V.
Bergstrom, L.
Berti, E.
Bigongiari, G.
Bobkov, S. G.
Boezio, M.
Bogomolov, E. A.
Bonechi, L.
Bongi, M.
Bottai, S.
Castellini, G.
Cattaneo, P. W.
Cumani, P.
Dalkarov, D.
Dedenko, G. L.
De Donato, C.
Dogiel, V. A.
Finetti, N.
Gascon, D.
Gorbunov, M. S.
Gusakov, Yu V.
Hnatyk, B. I.
Kadilin, V. V.
Kaplin, V. A.
Kaplun, A. A.
Kheymits, M. D.
Korepanov, V. E.
Larsson, J.
Leonov, A. A.
Loginov, V. A.
Longo, F.
Maestro, P.
Marrocchesi, P. S.
Martinez, M.
Men'shenin, A. L.
Mikhailov, V. V.
Mocchiutti, E.
Moiseev, A. A.
Mori, N.
Moskalenko, I. V.
Naumov, P. Yu
Papini, P.
Paredes, J. M.
Pearce, M.
Picozza, P.
Rappoldi, A.
Ricciarini, S.
Runtso, M. F.
Ryde, F.
Serdin, O. V.
Sparvoli, R.
Spillantini, P.
Stozhkov, Yu I.
Suchkov, S. I.
Taraskin, A. A.
Tavani, M.
Tiberio, A.
Tyurin, E. M.
Ulanov, M. V.
Vacchi, A.
Vannuccini, E.
Vasilyev, G. I.
Ward, J. E.
Yurkin, Yu T.
Zampa, N.
Zirakashvili, V. N.
Zverev, V. G.
GP IOP
TI The GAMMA-400 gamma-ray telescope for precision gamma-ray emission
investigations
SO INTERNATIONAL CONFERENCE ON PARTICLE PHYSICS AND ASTROPHYSICS
(ICPPA-2015), PTS 1-4
SE Journal of Physics Conference Series
LA English
DT Proceedings Paper
CT International Conference on Particle Physics and Astrophysics (ICPPA)
CY OCT 05-10, 2015
CL Moscow, RUSSIA
SP Natl Res Nucl Univ MEPhI, Ctr Fundamental Res & Particle Phys
AB The GAMMA-400 gamma-ray telescope with excellent angular and energy resolutions is designed to search for signatures of dark matter in the fluxes of gamma-ray emission and electrons + positrons. Precision investigations of gamma-ray emission from Galactic Center, Crab, Vela, Cygnus, Geminga, and other regions will be performed, as well as diffuse gamma-ray emission, along with measurements of high-energy electron + positron and nuclei fluxes. Furthermore, it will study gamma-ray bursts and gamma-ray emission from the Sun during periods of solar activity. The GAMMA-400 energy range is expected to be from similar to 20 MeV up to TeV energies for gamma rays, up to 10 TeV for electrons + positrons, and up to 10(15) eV for cosmic-ray nuclei. For 100-GeV gamma rays, the GAMMA-400 angular resolution is similar to 0.01 degrees and energy resolution is similar to 1%; the proton rejection factor is similar to 5x10(5). GAMMA-400 will be installed onboard the Russian space observatory.
C1 [Topchiev, N. P.; Galper, A. M.; Dalkarov, D.; Dogiel, V. A.; Gusakov, Yu V.; Leonov, A. A.; Stozhkov, Yu I.; Suchkov, S. I.] PN Lebedev Phys Inst, RU-119991 Moscow, Russia.
[Galper, A. M.; Arkhangelskaja, I. V.; Arkhangelskiy, A. I.; Bakaldin, A. V.; Dedenko, G. L.; Kadilin, V. V.; Kaplin, V. A.; Kaplun, A. A.; Kheymits, M. D.; Leonov, A. A.; Loginov, V. A.; Mikhailov, V. V.; Naumov, P. Yu; Runtso, M. F.; Taraskin, A. A.; Tyurin, E. M.; Yurkin, Yu T.; Zverev, V. G.] Natl Res Nucl Univ, MEPhI, Moscow Engn Phys Inst, Kashirskoe Highway 31, Moscow 115409, Russia.
[Bonvicini, V.; Boezio, M.; Cumani, P.; Longo, F.; Mocchiutti, E.; Vacchi, A.; Zampa, N.] Ist Nazl Fis Nucl, Sez Trieste, I-34149 Trieste, Italy.
[Adriani, O.; Berti, E.; Bongi, M.; Bottai, S.; Finetti, N.; Mori, N.; Papini, P.; Spillantini, P.; Tiberio, A.; Vannuccini, E.] Ist Nazl Fis Nucl, Sez Florence, I-50019 Florence, Italy.
[Aptekar, R. L.; Bogomolov, E. A.; Ulanov, M. V.; Vasilyev, G. I.] AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia.
[Bergstrom, L.] Stockholm Univ, AlbaNova Univ Ctr, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bigongiari, G.; Bonechi, L.; Maestro, P.; Marrocchesi, P. S.] Univ Siena, Dept Phys Sci Earth & Environm, I-53100 Siena, Italy.
[Bigongiari, G.; Bonechi, L.; Maestro, P.; Marrocchesi, P. S.] Ist Nazl Fis Nucl, Sez Pisa, Pisa, Italy.
[Bobkov, S. G.; Gorbunov, M. S.; Serdin, O. V.] Sci Res Inst Syst Anal, RU-117218 Moscow, Russia.
[Castellini, G.; Ricciarini, S.] Ist Fis Applicata Nello Carrara, I-50019 Florence, Italy.
[Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy.
[De Donato, C.; Picozza, P.; Sparvoli, R.] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, I-00133 Rome, Italy.
[Gascon, D.; Paredes, J. M.] Univ Barcelona, Dept Astron & Meteorol, Inst Ciencies Cosmos, E-08007 Barcelona, Spain.
[Hnatyk, B. I.] Taras Shevchenko Natl Univ, UA-01601 Kiev, Ukraine.
[Korepanov, V. E.] Lviv Ctr Inst Space Res, UA-79060 Lvov, Ukraine.
[Larsson, J.; Pearce, M.; Ryde, F.] Alballova Univ Ctr, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, J.; Pearce, M.; Ryde, F.] Alballova Univ Ctr, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Cumani, P.; Martinez, M.; Ward, J. E.] Inst Fis Altes Energies, Bellaterra, Spain.
[Men'shenin, A. L.] Res Inst Electromech, RU-143502 Istra, Moscow Region, Russia.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] Univ Maryland, CRESST, Greenbelt, MD 20771 USA.
[Moskalenko, I. V.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Moskalenko, I. V.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Tavani, M.] Univ Roma Tor Vergata, Ist Nazl Astrofis IASF, I-00133 Rome, Italy.
[Tavani, M.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy.
[Zirakashvili, V. N.] Pushkov Inst Terr Magnetism Ionosphere & Radiowav, Troitsk, Moscow Region, Russia.
RP Topchiev, NP (reprint author), PN Lebedev Phys Inst, RU-119991 Moscow, Russia.
EM tnp51@yandex.ru
RI DALKAROV, OLEG/E-1049-2014; Bobkov, Sergey/S-8153-2016; Vacchi,
Andrea/C-1291-2010; Mori, Nicola/D-9459-2016; Mikhailov,
Vladimir/B-5368-2014; Архангельский, Андрей/O-3676-2016; Leonov,
Alexey/E-4698-2016; Suchkov, Sergey/M-6671-2015; Stozhkov,
Yuri/M-7433-2015; Moskalenko, Igor/A-1301-2007; Galper,
Arkady/M-9610-2015; Dogiel, Vladimir/G-1450-2014; Topchiev,
Nikolay/M-6670-2015; Vasilyev, Gennady/E-4843-2014; Gorbunov,
Maxim/M-4484-2013; De Donato, Cinzia/J-9132-2015
OI Ricciarini, Sergio Bruno/0000-0001-6176-3368; Vacchi,
Andrea/0000-0003-3855-5856; Boezio, Mirko/0000-0002-8015-2981; Mori,
Nicola/0000-0003-2138-3787; Mikhailov, Vladimir/0000-0003-3851-2901;
Архангельский, Андрей/0000-0001-6406-6736; Moskalenko,
Igor/0000-0001-6141-458X; Topchiev, Nikolay/0000-0002-2875-8978;
Gorbunov, Maxim/0000-0002-4017-7033; De Donato,
Cinzia/0000-0002-9725-1281
NR 22
TC 0
Z9 0
U1 8
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1742-6588
J9 J PHYS CONF SER
PY 2016
VL 675
AR 032009
DI 10.1088/1742-6596/675/3/032009
PG 6
WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA BE5AH
UT WOS:000372460100075
ER
PT J
AU Ordaz, I
Li, W
AF Ordaz, Irian
Li, Wu
TI Approximation of Off-Body Sonic-Boom Analysis for Low-Boom Conceptual
Design
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID SUPERSONIC AIRCRAFT; INVERSE DESIGN; OPTIMIZATION; PREDICTION
AB The conceptual design of a low-boom and low-drag supersonic aircraft remains a challenge despite significant progress in recent years. Inverse design using reversed equivalent area and adjoint methods has been demonstrated to be effective in shaping the ground signature propagated from computational fluid dynamics off-body-pressure distributions. However, there is still a need to reduce the computational cost in the early stages of design to obtain a baseline that is feasible for low-boom shaping, and in the search for a robust low-boom design over the entire sonic-boom footprint. The proposed design method addresses the need to reduce the computational cost for robust low-boom design by using surface-pressure distributions from computational fluid dynamics solutions to shape sonic-boom ground signatures propagated from computational fluid dynamics off-body pressure.
C1 [Ordaz, Irian; Li, Wu] NASA, Aeronaut Syst Anal Branch, Syst Anal & Concepts Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
RP Ordaz, I (reprint author), NASA, Aeronaut Syst Anal Branch, Syst Anal & Concepts Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
FU Copyright Clearance Center, Inc., Rosewood Drive, Danvers
FX This material is declared a work of the U.S. Government and is not
subject to copyright protection in the United States. Copies of this
paper may be made for personal or internal use, on condition that the
copier pay the $10.00 per-copy fee to the Copyright Clearance Center,
Inc., 222 Rosewood Drive, Danvers, MA01923; include the code
1533-3868/15 and $10.00 in correspondence with the CCC.
NR 18
TC 0
Z9 0
U1 3
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN-FEB
PY 2016
VL 53
IS 1
BP 14
EP 19
DI 10.2514/1.C033159
PG 6
WC Engineering, Aerospace
SC Engineering
GA DH5BF
UT WOS:000372799300001
ER
PT J
AU Yeo, H
Potsdam, M
AF Yeo, Hyeonsoo
Potsdam, Mark
TI Rotor Structural Loads Analysis Using Coupled Computational Fluid
Dynamics/Computational Structural Dynamics
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID COMPREHENSIVE ANALYSIS; PREDICTION; AIRLOADS; PERFORMANCE; HELICOPTER
AB Coupled computational fluid dynamics/computational structural dynamics (RCAS/HELIOS and CAMRAD II/HELIOS) analyses are performed, and the calculated rotor structural loads are compared with the flight-test data obtained from the NASA/Army UH-60A Airloads Program. Three challenging level-flight conditions are investigated: 1) high speed with advancing blade negative lift, 2) low speed with blade/wake interaction, and 3) high thrust with dynamic stall. The predicted flap bending and torsion moments, pitch link, and lag damper loads, in general, show reasonably good correlation with the test data. A nonlinear lag damper model is essential for the accurate prediction of root chord bending moment and lag damper load. Both analyses, however, significantly underpredict the chord bending moments, especially the 4/rev harmonic amplitude. Parametric study shows that blade stiffness variations have only a small influence on the load calculations. However, modal damping in the first flap mode has a significant influence on the flap bending moments.
C1 [Yeo, Hyeonsoo; Potsdam, Mark] US Army Aviat Dev Directorate AFDD, Ames Res Ctr, Aviat & Missile Res Dev & Engn Ctr, Moffett Field, CA 94035 USA.
[Yeo, Hyeonsoo; Potsdam, Mark] US Army Aviat Dev Directorate AFDD, Ames Res Ctr, Res Dev & Engn Command, Moffett Field, CA 94035 USA.
RP Yeo, H (reprint author), US Army Aviat Dev Directorate AFDD, Ames Res Ctr, Aviat & Missile Res Dev & Engn Ctr, Moffett Field, CA 94035 USA.; Yeo, H (reprint author), US Army Aviat Dev Directorate AFDD, Ames Res Ctr, Res Dev & Engn Command, Moffett Field, CA 94035 USA.
EM hyeonsoo.yeo.civ@mail.mil; mark.a.potsdam.civ@mail.mil
FU Copyright Clearance Center, Inc. Rosewood Drive, Danvers, MA
FX This material is declared a work of the U.S. Government and is not
subject to copyright protection in the United States. Copies of this
paper may be made for personal or internal use, on condition that the
copier pay the $10.00 per-copy fee to the Copyright Clearance Center,
Inc., 222 Rosewood Drive, Danvers, MA 01923; include the code
1533-3868/15 and $10.00 in correspondence with the CCC.
NR 30
TC 1
Z9 1
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN-FEB
PY 2016
VL 53
IS 1
BP 87
EP 105
DI 10.2514/1.C033194
PG 19
WC Engineering, Aerospace
SC Engineering
GA DH5BF
UT WOS:000372799300007
ER
PT J
AU Rizzi, SA
Stephens, DB
Berton, JJ
Van Zante, DE
Wojno, JP
Goerig, TW
AF Rizzi, Stephen A.
Stephens, David B.
Berton, Jeffrey J.
Van Zante, Dale E.
Wojno, John P.
Goerig, Trevor W.
TI Auralization of Flyover Noise from Open-Rotor Engines Using Model-Scale
Test Data
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB A series of model-scale tests were recently completed using the open-rotor propulsion rig at the NASA John H. Glenn Research Center at Lewis Field in an effort to characterize the aeroacoustic performance of several open-rotor-propulsor designs. These included the historical-baseline and second-generation blade sets. Subsequently, the second generation design was assessed to have significant cumulative margins relative to the International Civil Aviation Organization Chapter 4 noise regulations, whilst the historical blade set had a negative margin. However, integrated metrics, like effective perceived-noise level, are not intuitive to the layperson, and likely do not convey the noise benefits over earlier designs, for example, the acoustically unique unducted-fan demonstrator of the 1980s. This paper develops the means of auralizing flyover-noise projections of full scale open-rotor engines using model-scale data in a manner that more readily communicates the noise benefit, and that is consistent with previously published aircraft-system-noise assessments. The effects of thrust level, installation type, and rotor-inflow angle on the generated flyover noise are investigated for the historical-baseline blade set. Finally, the benefits of the modern open-rotor blade design are made apparent through comparison of flyover noise from the second-generation and historical-baseline blade sets.
C1 [Rizzi, Stephen A.] NASA, Langley Res Ctr, Aeroacoust Branch, Aeroacoust, MS 463, Hampton, VA 23681 USA.
[Stephens, David B.; Van Zante, Dale E.] NASA, John H Glenn Res Ctr, Lewis Field, Acoust Branch, MS 54-3, Cleveland, OH 44135 USA.
[Berton, Jeffrey J.] NASA, John H Glenn Res Ctr, Lewis Field, Multidisciplinary Design Anal & Optimizat Branch, MS 5-11, Cleveland, OH 44135 USA.
[Wojno, John P.; Goerig, Trevor W.] GE Aviat, Acoust & Installat Aerodynam, 1 Neumann Way, Cincinnati, OH 45215 USA.
RP Rizzi, SA (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Aeroacoust, MS 463, Hampton, VA 23681 USA.
FU Environmentally Responsible Aviation project of the NASA Integrated
Systems Research Program; Fixed Wing and Aeronautical Sciences Projects
of the NASA Fundamental Aeronautics Program
FX This work was performed with support from the Environmentally
Responsible Aviation project of the NASA Integrated Systems Research
Program and the Fixed Wing and Aeronautical Sciences Projects of the
NASA Fundamental Aeronautics Program. The GE Open Rotor blade design and
testing were accomplished under the support of the Federal Aviation
Administration's Continuous Lower Energy, Emissions and Noise program.
NR 31
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN-FEB
PY 2016
VL 53
IS 1
BP 117
EP 128
DI 10.2514/1.C033223
PG 12
WC Engineering, Aerospace
SC Engineering
GA DH5BF
UT WOS:000372799300009
ER
PT J
AU Glaze, LS
Baloga, SM
AF Glaze, Lori S.
Baloga, Stephen M.
TI Simulation of cooling and pressure effects on inflated pahoehoe lava
flows
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID KILAUEA VOLCANO; FLOOD LAVAS; HAWAII; MODEL; EMPLACEMENT; DYNAMICS
AB Pahoehoe lobes are often emplaced by the advance of discrete toes accompanied by inflation of the lobe surface. Many random effects complicate modeling lobe emplacement, such as the location and orientation of toe breakouts, their dimensions, mechanical strength of the crust, microtopography, and a host of other factors. Models that treat the movement of lava parcels as a random walk have explained some of the overall features of emplacement. However, cooling of the surface and internal pressurization of the fluid interior have not been modeled. This work reports lobe simulations that explicitly incorporate (1) cooling of surface lava parcels, (2) the propensity of breakouts to occur at warmer margins that are mechanically weaker than cooler ones, and (3) the influence of internal pressurization associated with inflation. The surface temperature is interpreted as a surrogate for the mechanic strength of the crust at each location and is used to determine the probability of a lava parcel transfer from that location. When only surface temperature is considered, the morphology and dimensions of simulated lobes are indistinguishable from equiprobable simulations. However, inflation within a lobe transmits pressure to all connected fluid locations with the warmer margins being most susceptible to breakouts and expansion. Simulations accounting for internal pressurization feature morphologies and dimensions that are dramatically different from the equiprobable and temperature-dependent models. Even on flat subsurfaces the pressure-dependent model produces elongate lobes with distinct directionality. Observables such as topographic profiles, aspect ratios, and maximum extents should be readily distinguishable in the field.
C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baloga, Stephen M.] Proxemy Res, Laytonville, MD USA.
RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Lori.S.Glaze@nasa.gov
RI Glaze, Lori/D-1314-2012
FU NASA Planetary Geology and Geophysics [WBS 811073.02.01.05.80, WBS
8110073.02.01.06.60, NNX13AR12G]
FX The authors would like to thank S. Rowland, D. Crown, A. Harris, S.
Self, T. Thordarson, and C. Hamilton for numerous detailed discussions
of pahoehoe emplacement observations. This work was conducted under NASA
Planetary Geology and Geophysics grants WBS 811073.02.01.05.80 and WBS
8110073.02.01.06.60 for LSG and NNX13AR12G for SMB. Simulation results
used to generate figures in this paper are available upon request.
NR 35
TC 0
Z9 0
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD JAN
PY 2016
VL 121
IS 1
BP 38
EP 47
DI 10.1002/2015JB012383
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DH8UU
UT WOS:000373073200004
ER
PT J
AU Boullot, N
Rabier, F
Langland, R
Gelaro, R
Cardinali, C
Guidard, V
Bauer, P
Doerenbecher, A
AF Boullot, Nathalie
Rabier, Florence
Langland, Rolf
Gelaro, Ron
Cardinali, Carla
Guidard, Vincent
Bauer, Peter
Doerenbecher, Alexis
TI Observation impact over the southern polar area during the Concordiasi
field campaign
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE dropsondes; forecast sensitivity to observations; observing-system
experiment; forecast score
ID RADIATION DRY BIAS; DATA ASSIMILATION; SCHEME; SYSTEM
AB The impact of observations on analysis uncertainty and forecast performance was investigated for austral spring 2010 over the southern polar area for four different systems (NRL, GMAO, ECMWF and Meteo-France) at the time of the Concordiasi field experiment. The largest multi-model variance in 500 hPa height analyses is found in the southern sub-Antarctic oceanic region, where there are rapidly evolving weather systems, rapid forecast-error growth, and fewer upper-air wind observation data to constrain the analyses. The total impact of all observations on the model forecast was computed using the 24 h forecast sensitivity-to-observations diagnostic. Observation types that contribute most to the reduction of the forecast error are shown to be AMSU, IASI, AIRS, GPS-RO, radiosonde, surface and atmospheric motion vector observations. For sounding data, radiosondes and dropsondes, one can note a large impact on the analysis and forecasts of temperature at low levels and a large impact of wind at high levels. Observing system experiments using the Concordiasi dropsondes show a large impact of the observations over the Antarctic plateau extending to lower latitudes with the forecast range, with the largest impact around 50-70 degrees S. These experiments indicate there is a potential benefit from using radiance data better over land and sea-ice and from innovative atmospheric motion vectors obtained from a combination of various satellites to fill the current data gaps and improve numerical weather prediction analyses in this region.
C1 [Boullot, Nathalie; Rabier, Florence; Guidard, Vincent; Doerenbecher, Alexis] Meteo France, CNRS, GAME, CNRM, 42 Ave Coriolis, F-31057 Toulouse 1, France.
[Rabier, Florence; Cardinali, Carla; Bauer, Peter] European Ctr Medium Range Weather Forecasts, Reading, Berks, England.
[Langland, Rolf] US Navy, Res Lab, Monterey, CA USA.
[Gelaro, Ron] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
RP Boullot, N (reprint author), Meteo France, CNRM GMAP, 42 Ave Coriolis, F-31057 Toulouse 1, France.
EM nathalie.boullot@meteo.fr
FU Meteo-France; CNES; CNRS/INSU; NSF; NCAR; University of Wyoming; Purdue
University; University of Colorado; Alfred Wegener Institute; Met
Office; ECMWF; IPEV; PNRA; USAP; BAS
FX Concordiasi is an international project, supported by the following
agencies: Meteo-France, CNES, CNRS/INSU, NSF, NCAR, University of
Wyoming, Purdue University, University of Colorado, the Alfred Wegener
Institute, the Met Office and ECMWF. Concordiasi also benefits from
logistic or financial support of the operational polar agencies IPEV,
PNRA, USAP and BAS, and from BSRN measurements at Concordia. Concordiasi
is part of the THORPEX-IPY cluster within the International Polar Year
effort. The authors would like to acknowledge Cihan Sahin (ECMWF) for
providing the singular vectors optimised over the southern polar area
during the Concordiasi experiment.
NR 23
TC 5
Z9 5
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JAN
PY 2016
VL 142
IS 695
BP 597
EP 610
DI 10.1002/qj.2470
PN B
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7DJ
UT WOS:000372951300007
ER
PT J
AU Ngodock, H
Carrier, M
Souopgui, I
Smith, S
Martin, P
Muscarella, P
Jacobs, G
AF Ngodock, Hans
Carrier, Matthew
Souopgui, Innocent
Smith, Scott
Martin, Paul
Muscarella, Philip
Jacobs, Gregg
TI On the direct assimilation of along-track sea-surface height
observations into a free-surface ocean model using a weak constraints
four-dimensional variational (4D-Var) method
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE data assimilation; along-track SSH; weak constraints 4D-Var; representer
method
ID PACIFIC-OCEAN; INDIAN-OCEAN; 4DVAR SYSTEM; MONTEREY BAY; PART II; WAVES;
PROPAGATION; LEVEL; SIMULATIONS; DYNAMICS
AB The representer method is adopted for solving a weak constraints 4D-Var problem for the assimilation of ocean observations including along-track sea-surface height (SSH), using a free-surface ocean model. Direct 4D-Var assimilation of SSH observations along the satellite tracks requires that the adjoint model be integrated with Dirac impulses on the right-hand side (rhs) of the adjoint equations for the surface elevation equation. The solution of this adjoint model will inevitably include surface gravity waves, and it constitutes the forcing for the tangent linear model (TLM) according to the representer method. This yields an analysis that is contaminated by gravity waves. A method for avoiding the generation of the surface gravity waves in the analysis is proposed in this study; it consists of removing the adjoint of the free surface from the rhs of the free-surface mode in the TLM. The information from the SSH observations will still propagate to all other variables via the adjoint of the balance relationship between the barotropic and baroclinic modes, resulting in the correction to the surface elevation. Two assimilation experiments are carried out in the Gulf of Mexico: one with adjoint forcing included on the rhs of the TLM free-surface equation, and the other without. Both analyses are evaluated against the assimilated SSH observations, SSH maps from AVISO and independent surface drifters, showing that the analysis that did not include adjoint forcing in the free surface is more accurate. This study shows that when a weak constraints 4D-Var approach is considered for the assimilation of along-track SSH observations using a free-surface model, with the aim of correcting the mesoscale circulation, an independent model error should not be assigned to the free surface.
C1 [Ngodock, Hans; Carrier, Matthew; Smith, Scott; Martin, Paul; Muscarella, Philip; Jacobs, Gregg] US Navy, Res Lab, Stennis Space Ctr, Mississippi State, MS USA.
[Souopgui, Innocent] Univ So Mississippi, Stennis Space Ctr, Dept Marine Sci, Hattiesburg, MS 39406 USA.
RP Ngodock, H (reprint author), 1009 Balch Blvd, Stennis Space Ctr, MS 39529 USA.
EM hans.ngodock@nrlssc.navy.mil
FU Office of Naval Research as part of 'Amultiscale Approach for Assessing
Predictability of ASW environment' [0601153N]; 'NCOM-4DVAR'
FX This work was sponsored by the Office of Naval Research, Program Element
0601153N, as part of 'Amultiscale Approach for Assessing Predictability
of ASW environment' and the 'NCOM-4DVAR' projects. This article is NRL
paper contribution number NRL/JA/7320-14-2148. The authors would like to
thank the anonymous reviewers; their comments helped in improving the
quality of this article.
NR 53
TC 1
Z9 1
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JAN
PY 2016
VL 142
IS 695
BP 1160
EP 1170
DI 10.1002/qj.2721
PN B
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH7DJ
UT WOS:000372951300052
ER
PT J
AU Guo, HQ
Meador, MAB
McCorkle, LS
Scheiman, DA
McCrone, JD
Wilkewitz, B
AF Guo, Haiquan
Meador, Mary Ann B.
McCorkle, Linda S.
Scheiman, Daniel A.
McCrone, Jordan D.
Wilkewitz, Brittany
TI Poly(maleic anhydride) cross-linked polyimide aerogels: synthesis and
properties
SO RSC ADVANCES
LA English
DT Article
ID MECHANICALLY STRONG
AB A series of aerogels was fabricated by cross-linking amine end-capped polyimide oligomers with poly(maleic anhydride) s. Poly(maleic anhydride) s are commercially available with various aliphatic side groups and are less costly than other cross-linkers used for polyimide aerogels. Thus they are used here as possible substitutes to form cross-linked polyimide aerogels at a lower cost. The effects of the different side groups of the cross-linkers and oligomer backbone structures on the density, porosity, shrinkage, surface area, morphology, and mechanical properties of the aerogels are discussed. Aerogels with low density (0.12-0.17 g cm(-3)), high porosity (>88%), high surface area (360-550 m(2) g(-1)), and Young's modulus (2-60 MPa) were produced in the study. The thermal stability and water uptake of the samples were also studied. The aerogels may be potential candidates in a variety of aeronautic and space applications, such as space suit insulation for planetary surface missions, insulation for inflatable structures for habitats, and cryotank insulation for advanced space propulsion systems.
C1 [Guo, Haiquan; McCorkle, Linda S.; Scheiman, Daniel A.] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
[Meador, Mary Ann B.; Wilkewitz, Brittany] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
[McCrone, Jordan D.] Vantage Partners LLC, Brighton, MA USA.
RP Guo, HQ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.; Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM haiquan.n.guo@nasa.gov; maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
FU Center Institutional Capabilities and ETD GCD Entry system modelling
Programs
FX We gratefully acknowledge support from the Center Institutional
Capabilities and ETD GCD Entry system modelling Programs. We thank
Baochau N. Nguyen, Ohio Aerospace Institute for NMR spectra. We also
thank the NASA Lewis' Educational and Research Collaborative Internship
Project (LERSIP) intern student program.
NR 29
TC 2
Z9 3
U1 8
U2 21
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2046-2069
J9 RSC ADV
JI RSC Adv.
PY 2016
VL 6
IS 31
BP 26055
EP 26065
DI 10.1039/c6ra01013j
PG 11
WC Chemistry, Multidisciplinary
SC Chemistry
GA DH5FV
UT WOS:000372812300050
ER
PT J
AU Klimchuk, JA
Patsourakos, S
Tripathi, D
AF Klimchuk, J. A.
Patsourakos, S.
Tripathi, D.
TI Intensity Conserving Spectral Fitting
SO SOLAR PHYSICS
LA English
DT Article
DE Instrumental effects; Spectral line, intensity and diagnostics; Active
regions, velocity field; Corona, active
ID EUV IMAGING SPECTROMETER; LINE-PROFILE ASYMMETRIES; ACTIVE-REGION
OUTFLOWS; SPECTROSCOPIC OBSERVATIONS; CHROMOSPHERIC NANOFLARES; SPLINE
INTERPOLATION; CORONAL PLASMA; SOLAR CORONA; HINODE; LOOPS
AB The detailed shapes of spectral-line profiles provide valuable information about the emitting plasma, especially when the plasma contains an unresolved mixture of velocities, temperatures, and densities. As a result of finite spectral resolution, the intensity measured by a spectrometer is the average intensity across a wavelength bin of non-zero size. It is assigned to the wavelength position at the center of the bin. However, the actual intensity at that discrete position will be different if the profile is curved, as it invariably is. Standard fitting routines (spline, Gaussian, etc.) do not account for this difference, and this can result in significant errors when making sensitive measurements. We have developed an iterative procedure that corrects for this effect. It converges rapidly and is very flexible in that it can be used with any fitting function. We present examples of cubic-spline and Gaussian fits and give special attention to measurements of blue-red asymmetries of coronal emission lines.
C1 [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
[Patsourakos, S.] Univ Ioannina, Dept Phys, GR-45110 Ioannina, Greece.
[Tripathi, D.] Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India.
RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
EM James.A.Klimchuk@nasa.gov; spatsourakos@gmail.com; durgesh@iucaa.in
OI Tripathi, Durgesh/0000-0003-1689-6254
FU NASA; FP7 Marie Curie Grant [FP7-PEOPLE-2010-RG/268288]; European Union;
Greek national government through the Operational Program "Education and
Lifelong Learning" of the National Strategic Reference Framework (NSRF)
Research Funding Program "Thales: Investing in knowledge society through
the European Social Fund"
FX This work of J.A. Klimchuk was supported by the NASA Supporting Research
and Technology Program. The work of S. Patsourakos was supported by an
FP7 Marie Curie Grant (FP7-PEOPLE-2010-RG/268288) and jointly by the
European Union and Greek national government through the Operational
Program "Education and Lifelong Learning" of the National Strategic
Reference Framework (NSRF) Research Funding Program "Thales: Investing
in knowledge society through the European Social Fund." D. Tripathi
acknowledges the Max-Planck Partner Group of MPS at IUCAA. The authors
benefited from participation in the International Space Science
Institute team on Using Observables to Settle the Question of Steady vs.
Impulsive Coronal Heating, led by Stephen Bradshaw and Helen Mason. We
thank the referee for comments that resulted in an improved manuscript.
NR 25
TC 2
Z9 2
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD JAN
PY 2016
VL 291
IS 1
BP 55
EP 65
DI 10.1007/s11207-015-0827-4
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH6CH
UT WOS:000372878100004
ER
PT J
AU Wu, CC
Lepping, RP
AF Wu, Chin-Chun
Lepping, Ronald P.
TI Relationships Among Geomagnetic Storms, Interplanetary Shocks, Magnetic
Clouds, and Sunspot Number During 1995-2012
SO SOLAR PHYSICS
LA English
DT Article
DE Geomagnetic storms; Interplanetary shocks; Magnetic clouds; Solar
activity; Solar cycle; Space weather
ID SOLAR-WIND; 1 AU; INTENSITY; CMES
AB During 1995-2012, the Wind spacecraft has recorded 168 magnetic clouds (MCs), 197 magnetic cloud-like structures (MCLs), and 358 interplanetary (IP) shocks. Ninety-four MCs and 56 MCLs had upstream shock waves. The following features are found: i) The averages of the solar wind speed, interplanetary magnetic field (IMF), duration (), the minimum of B-min, and intensity of the associated geomagnetic storm/activity (Dst(min)) for MCs with upstream shock waves (MCshock) are higher (or stronger) than those averages for the MCs without upstream shock waves (MCno-shock). ii) The average of MCshock events (approximate to 19.8 h) is 9% longer than that for MCno-shock events (approximate to 17.6 h). iii) For the MCshock events, the average duration of the sheath () is 12.1 h. These findings could be very useful for space weather predictions, i.e. IP shocks driven by MCs are expected to arrive at Wind (or at 1 AU) about 12 h ahead of the front of the MCs on average. iv) The occurrence frequency of IP shocks is well associated with sunspot number (SSN). The average intensity of geomagnetic storms measured by < Dst(min)> for MCshock and MCno-shock events is -102 and -31 nT, respectively. The average values < Dst(min)> are -78, -70, and -35 nT for the 358 IP shocks, 168 MCs, and 197 MCLs, respectively. These results imply that IP shocks, when they occur with MCs/MCLs, must play an important role in the strength of geomagnetic storms. We speculate about the reason for this. Yearly occurrence frequencies of MCshock and IP shocks are well correlated with solar activity (e.g., SSN). Choosing the correct Dst(min) estimating formula for predicting the intensity of MC-associated geomagnetic storms is crucial for space weather predictions.
C1 [Wu, Chin-Chun] Naval Res Lab, Washington, DC 20375 USA.
[Lepping, Ronald P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Wu, CC (reprint author), Naval Res Lab, Washington, DC 20375 USA.
EM Chin-Chun.Wu@nrl.navy.mil
FU NASA [NNX13AI75G]
FX We are grateful to the Wind SWE and MFI teams, Kyoto University (Dst
data), the World Data Center SILSO of the Royal Observatory of Belgium
(sunspot number), NOAA/NGDC (which provided web access for sunspot
number and Dst data sets), and the Harvard-Smithsonian Center for
Astrophysics Interplanetary Shock Database (supported by NASA grant
number NNX13AI75G) for the use of their data. Work of CCW is supported
by the Chief of Naval Research.
NR 26
TC 7
Z9 7
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD JAN
PY 2016
VL 291
IS 1
BP 265
EP 284
DI 10.1007/s11207-015-0806-9
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH6CH
UT WOS:000372878100015
ER
PT J
AU Pesnell, WD
AF Pesnell, William Dean
TI Predictions of Solar Cycle 24: How are we doing?
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID MAGNETIC-FIELD REVERSAL; GROUP SUNSPOT NUMBERS; POLAR CORONAL HOLE;
ACTIVITY RECONSTRUCTION; PRECURSOR METHOD; DYNAMO MODEL; AMPLITUDE;
MAXIMUM; PARAMETERS; FORECAST
AB Predictions of solar activity are an essential part of our Space Weather forecast capability. Users are requiring usable predictions of an upcoming solar cycle to be delivered several years before solar minimum. A set of predictions of the amplitude of Solar Cycle 24 accumulated in 2008 ranged from zero to unprecedented levels of solar activity. The predictions formed an almost normal distribution, centered on the average amplitude of all preceding solar cycles. The average of the current compilation of 105 predictions of the annual-average sunspot number is 106 +/- 31, slightly lower than earlier compilations but still with a wide distribution. Solar Cycle 24 is on track to have a below-average amplitude, peaking at an annual sunspot number of about 80. Our need for solar activity predictions and our desire for those predictions to be made ever earlier in the preceding solar cycle will be discussed. Solar Cycle 24 has been a below-average sunspot cycle. There were peaks in the daily and monthly averaged sunspot number in the Northern Hemisphere in 2011 and in the Southern Hemisphere in 2014. With the rapid increase in solar data and capability of numerical models of the solar convection zone we are developing the ability to forecast the level of the next sunspot cycle. But predictions based only on the statistics of the sunspot number are not adequate for predicting the next solar maximum. I will describe how we did in predicting the amplitude of Solar Cycle 24 and describe how solar polar field predictions could be made more accurate in the future.
C1 [Pesnell, William Dean] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM william.d.pesnell@nasa.gov
RI Pesnell, William/D-1062-2012
OI Pesnell, William/0000-0002-8306-2500
FU NASA's Solar Dynamics Observatory; NASA
FX This work was supported by NASA's Solar Dynamics Observatory. The
international sunspot number values are from the WDC-SILSO, Royal
Observatory of Belgium, Brussels. F10.7 values are courtesy
of the Dominion Radio Astronomy Observatory, Penticton, British
Columbia, Canada and downloaded from the National Geophysical Data
Center (NGDC) in Boulder, Colorado. The polar magnetic field data are
from the Wilcox Solar Observatory (http://wso.stanford.edu/Polar.html)
and are courtesy of J. T. Hoeksema. The Wilcox Solar Observatory is
currently supported by NASA.
NR 63
TC 2
Z9 2
U1 1
U2 7
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 JAN
PY 2016
VL 14
IS 1
BP 10
EP 21
DI 10.1002/2015SW001304
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DH9NB
UT WOS:000373121700002
ER
PT J
AU Balikhin, MA
Rodriguez, JV
Boynton, RJ
Walker, SN
Aryan, H
Sibeck, DG
Billings, SA
AF Balikhin, M. A.
Rodriguez, J. V.
Boynton, R. J.
Walker, S. N.
Aryan, H.
Sibeck, D. G.
Billings, S. A.
TI Comparative analysis of NOAA REFM and SNB(3)GEO tools for the forecast
of the fluxes of high-energy electrons at GEO
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID SOLAR-WIND; GEOSYNCHRONOUS ORBIT; NONLINEAR MODELS; DST INDEX;
IDENTIFICATION; PREDICTION; SYSTEMS; SPACECRAFT; LOSSES; EVENT
AB Reliable forecasts of relativistic electrons at geostationary orbit (GEO) are important for the mitigation of their hazardous effects on spacecraft at GEO. For a number of years the Space Weather Prediction Center at NOAA has provided advanced online forecasts of the fluence of electrons with energy > 2 MeV at GEO using the Relativistic Electron Forecast Model (REFM). The REFM forecasts are based on real-time solar wind speed observations at L1. The high reliability of this forecasting tool serves as a benchmark for the assessment of other forecasting tools. Since 2012 the Sheffield SNB(3)GEO model has been operating online, providing a 24 h ahead forecast of the same fluxes. In addition to solar wind speed, the SNB(3)GEO forecasts use solar wind density and interplanetary magnetic field B-z observations at L1. The period of joint operation of both of these forecasts has been used to compare their accuracy. Daily averaged measurements of electron fluxes by GOES 13 have been used to estimate the prediction efficiency of both forecasting tools. To assess the reliability of both models to forecast infrequent events of very high fluxes, the Heidke skill score was employed. The results obtained indicate that SNB(3)GEO provides a more accurate 1 day ahead forecast when compared to REFM. It is shown that the correction methodology utilized by REFM potentially can improve the SNB(3)GEO forecast.
C1 [Balikhin, M. A.; Boynton, R. J.; Walker, S. N.; Billings, S. A.] Univ Sheffield, ACSE, Sheffield, S Yorkshire, England.
[Rodriguez, J. V.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Rodriguez, J. V.] NOAA, Natl Ctr Environm Informat, Boulder, CO USA.
[Aryan, H.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Balikhin, MA (reprint author), Univ Sheffield, ACSE, Sheffield, S Yorkshire, England.
EM m.balikhin@sheffield.ac.uk
FU ISSI; European Union's Horizon 2020 research and innovation programme
[637302]; EPSRC UK [EP/H00453X/1]; NASA Postdoctoral Program at Goddard
Space Flight Center; Van Allen Probes mission
FX M.A.B. would like to acknowledge financial support from ISSI. This
project has received funding from the European Union's Horizon 2020
research and innovation programme under grant agreement 637302. M.A.B.,
S.A.B., and R.J.B. would like to acknowledge financial support from
EPSRC UK, Platform grant EP/H00453X/1. H.A. would like to acknowledge
financial support from NASA Postdoctoral Program at Goddard Space Flight
Center. DGS acknowledges that portions of the work at NASA/GSFC were
funded by the Van Allen Probes mission. As mentioned in the text,
forecasts from the SNB3GEO model are available from
http://www.ssg.group.shef.ac.uk/USSW/Archive_EF/All/All_EF.html and the
GOES 13 Daily Particle Data (DPD) files from
ftp://ftp.swpc.noaa.gov/pub/indices/old_indices/. We thank H. Singer and
SWPC for providing the REFM model outputs. The REFM outputs are provided
as supporting information.
NR 45
TC 1
Z9 1
U1 2
U2 3
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 JAN
PY 2016
VL 14
IS 1
BP 22
EP 31
DI 10.1002/2015SW001303
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DH9NB
UT WOS:000373121700003
ER
PT J
AU Ishimatsu, T
de Weck, OL
Hoffman, JA
Ohkami, Y
Shishko, R
AF Ishimatsu, Takuto
de Weck, Olivier L.
Hoffman, Jeffrey A.
Ohkami, Yoshiaki
Shishko, Robert
TI Generalized Multicommodity Network Flow Model for the Earth-Moon-Mars
Logistics System
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB Simple logistics strategies such as "carry-along" and Earth-based "resupply" were sufficient for past human space programs. Next-generation space logistics paradigms are expected to be more complex, involving multiple exploration destinations and in situ resource utilization. Optional in situ resource utilization brings additional complexity to the interplanetary supply chain network design problem. This paper presents an interdependent network flow modeling method for determining optimal logistics strategies for space exploration and its application to the human exploration of Mars. It is found that a strategy using lunar resources in the cislunar network may improve overall launch mass to low Earth orbit for recurring missions to Mars compared to NASA's Mars Design Reference Architecture 5.0, even when including the mass of the in situ resource utilization infrastructures that need to be predeployed. Other findings suggest that chemical propulsion using liquid oxygen/liquid hydrogen, lunar in situ resource utilization water production, and the use of aerocapture significantly contribute to reducing launch mass from Earth. A sensitivity analysis of in situ resource utilization reveals that, under the given assumptions, local lunar resources become attractive at productivity levels above 1.8 kg/year/kg in the context of future human exploration of Mars.
C1 [Ishimatsu, Takuto] MIT, Engn Syst Div, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[de Weck, Olivier L.] MIT, Dept Aeronaut & Astronaut, Engn Syst Div, Cambridge, MA 02139 USA.
[Hoffman, Jeffrey A.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
[Ohkami, Yoshiaki] Keio Univ, Grad Sch Syst Design & Management, Kohoku Ku, 4-1-1 Hiyoshi, Yokohama, Kanagawa 2238526, Japan.
[Shishko, Robert] CALTECH, Jet Prop Lab, Project Syst Engn & Formulat Sect, M-S 301-160, Pasadena, CA 91109 USA.
RP Ishimatsu, T (reprint author), MIT, Engn Syst Div, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
FU NASA Jet Propulsion Laboratory through a Strategic University Research
Partnership grant
FX The research described in this paper was carried out at the
Massachusetts Institute of Technology (MIT) and was supported in part by
NASA Jet Propulsion Laboratory through a Strategic University Research
Partnership grant. The authors wish to acknowledge the support of Thomas
Coffee, Paul Grogan, and Koki Ho at MIT.
NR 32
TC 5
Z9 5
U1 3
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2016
VL 53
IS 1
BP 25
EP 38
DI 10.2514/1.A33235
PG 14
WC Engineering, Aerospace
SC Engineering
GA DH0IZ
UT WOS:000372469200003
ER
PT J
AU Gatsonis, NA
Lu, Y
Blandino, J
Demetriou, MA
Paschalidis, N
AF Gatsonis, Nikolaos A.
Lu, Ye
Blandino, John
Demetriou, Michael A.
Paschalidis, Nicholas
TI Micropulsed Plasma Thrusters for Attitude Control of a
Low-Earth-Orbiting CubeSat
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB This study presents a 3-Unit CubeSat design with commercial-off-the-shelf hardware, Teflon (R)-fueled micropulsed plasma thrusters, and an attitude determination and control approach. The micropulsed plasma thruster is sized by the impulse bit and pulse frequency required for continuous compensation of expected maximum disturbance torques at altitudes between 400 and 1000 km, as well as to perform stabilization of up to 20 deg / s and slewmaneuvers of up to 180 deg. The study involves realistic power constraints anticipated on the 3-Unit CubeSat. Attitude estimation is implemented using the q method for static attitude determination of the quaternion using pairs of the spacecraft-sun and magnetic-field vectors. The quaternion estimate and the gyroscope measurements are used with an extended Kalman filter to obtain the attitude estimates. Proportional-derivative control algorithms use the static attitude estimates in order to calculate the torque required to compensate for the disturbance torques and to achieve specified stabilization and slewing maneuvers or combinations. The controller includes a thruster-allocationmethod, which determines the optimal utilization of the available thrusters and introduces redundancy in case of failure. Simulation results are presented for a 3-Unit CubeSat under detumbling, pointing, and pointing and spinning scenarios, as well as comparisons between the thruster-allocation and the paired-firing methods under thruster failure.
C1 [Gatsonis, Nikolaos A.; Lu, Ye; Blandino, John; Demetriou, Michael A.] Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
[Paschalidis, Nicholas] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Gatsonis, NA (reprint author), Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
NR 36
TC 0
Z9 0
U1 5
U2 9
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2016
VL 53
IS 1
BP 57
EP 73
DI 10.2514/1.A33345
PG 17
WC Engineering, Aerospace
SC Engineering
GA DH0IZ
UT WOS:000372469200006
ER
PT J
AU Chen, YK
Gokcen, T
AF Chen, Yih-Kanq
Goekcen, Tahir
TI Evaluation of Finite-Rate Gas/Surface Interaction Models for
Carbon-Based Ablator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 15th AIAA Aviation Technology, Integration, and Operations Conference
CY JUN 22-26, 2015
CL Dallas, TX
SP AIAA
ID THERMAL RESPONSE; 2-DIMENSIONAL ABLATION; SHAPE CHANGE; SIMULATION;
PYROLYSIS; CHEMISTRY; ACETYLENE; KINETICS; SURFACE; FLOW
AB Two sets of finite-rate gas/surface interaction model between air and the carbon surface are studied. The first set is an engineering model with one-way chemical reactions, and the second set is a more detailed model with two-way chemical reactions. Each of these two proposed models intends to cover the carbon surface ablation conditions including the low-temperature rate-controlled oxidation, the midtemperature diffusion-controlled oxidation, and the high-temperature sublimation. The prediction of carbon surface recession is achieved by coupling a material thermal response code and a Navier-Stokes flow code. The material thermal response code used in this study is the Two-Dimensional Implicit Thermal-Response and Ablation Program, which predicts charring material thermal response and shape change on hypersonic space vehicles. The flow code solves the reacting full Navier-Stokes equations using the data parallel line relaxation method. Recession analyses of stagnation tests conducted in NASA Ames Research Center arc-jet facilities with heat fluxes ranging from 45 to 1100 W/cm(2) are performed and compared with data for model validation. The ablating material used in these arc-jet tests is phenolic impregnated carbon ablator. Computational predictions of surface recession and shape change are in good agreement with measurement for arc-jet conditions.
C1 [Chen, Yih-Kanq] NASA, Ames Res Ctr, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA.
[Goekcen, Tahir] ERC Inc, Moffett Field, CA 94035 USA.
RP Chen, YK (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA.
NR 27
TC 0
Z9 0
U1 3
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2016
VL 53
IS 1
BP 143
EP 152
DI 10.2514/1.A33377
PG 10
WC Engineering, Aerospace
SC Engineering
GA DH0IZ
UT WOS:000372469200012
ER
PT S
AU Burke, ER
DeHaven, SL
Williams, PA
AF Burke, E. R.
DeHaven, S. L.
Williams, P. A.
BE Chimenti, DE
Bond, LJ
TI Scintillating Quantum Dots for Imaging X-rays (SQDIX) for Aircraft
Inspection
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
AB Scintillation is the process currently employed by conventional X-ray detectors to create X-ray images. Scintillating quantum dots (StQDs) or nano-crystals are novel, nanometer-scale materials that upon excitation by X-rays, re-emit the absorbed energy as visible light. StQDs theoretically have higher output efficiency than conventional scintillating materials and are more environmentally friendly. This paper will present the characterization of several critical elements in the use of StQDs that have been performed along a path to the use of this technology in wide spread X-ray imaging. Initial work on the scintillating quantum dots for imaging X-rays (SQDIX) system has shown great promise to create state-of-the-art sensors using StQDs as a sensor material. In addition, this work also demonstrates a high degree of promise using StQDs in microstructured fiber optics. Using the microstructured fiber as a light guide could greatly increase the capture efficiency of a StQDs based imaging sensor.
C1 [Burke, E. R.; DeHaven, S. L.; Williams, P. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Burke, ER (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM eric.r.burke@nasa.gov; stanton.l.dehaven@nasa.gov;
phillip.a.williams@nasa.gov
NR 4
TC 0
Z9 0
U1 3
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 110007
DI 10.1063/1.4940578
PG 6
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800132
ER
PT S
AU Burke, ER
Grubsky, V
Romanov, V
Shoemaker, K
AF Burke, E. R.
Grubsky, V.
Romanov, V.
Shoemaker, K.
BE Chimenti, DE
Bond, LJ
TI NDE of Spacecraft Materials Using 3D Compton Backscatter X-Ray Imaging
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
AB We present the results of testing of the NDE performance of a Compton Imaging Tomography (CIT) system for single-sided, penetrating 3D inspection. The system was recently developed by Physical Optics Corporation (POC) and delivered to NASA for testing and evaluation. The CIT technology is based on 3D structure mapping by collecting the information on density profiles in multiple object cross sections through hard x-ray Compton backscatter imaging. The individual cross sections are processed and fused together in software, generating a 3D map of the density profile of the object which can then be analyzed slice-by-slice in x, y, or z directions. The developed CIT scanner is based on a 200-kV x-ray source, flat-panel x-ray detector (FPD), and apodized x-ray imaging optics. The CIT technology is particularly well suited to the NDE of lightweight aerospace materials, such as the thermal protection system (TPS) ceramic and composite materials, micrometeoroid and orbital debris (MMOD) shielding, spacecraft pressure walls, inflatable habitat structures, composite overwrapped pressure vessels (COPVs), and aluminum honeycomb materials. The current system provides 3D localization of defects and features with field of view 20x12x8 cm3 and spatial resolution similar to 2 mm. In this paper, we review several aerospace NDE applications of the CIT technology, with particular emphasis on TPS. Based on the analysis of the testing results, we provide recommendations for continued development on TPS applications that can benefit the most from the unique capabilities of this new NDE technology.
C1 [Burke, E. R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Grubsky, V.; Romanov, V.; Shoemaker, K.] Phys Opt Corp, 1845 W 205th St, Torrance, CA 90501 USA.
RP Burke, ER (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM eric.r.burke@nasa.gov; vgrubsky@poc.com; vromanov@poc.com;
kshoemaker@poc.com
NR 5
TC 0
Z9 0
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 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 110006
DI 10.1063/1.4940577
PG 5
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800131
ER
PT S
AU DeHaven, SL
Williams, PA
Burke, ER
AF DeHaven, S. L.
Williams, P. A.
Burke, E. R.
BE Chimenti, DE
Bond, LJ
TI Quantum Dots Microstructured Optical Fiber for X-ray Detection
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
AB A novel concept for the detection of x-rays with microstructured optical fibers containing quantum dots scintillation material comprised of zinc sulfide nanocrystals doped with magnesium sulfide is presented. These quantum dots are applied inside the microstructured optical fibers using capillary action. The x-ray photon counts of these fibers are compared to the output of a collimated CdTe solid state detector over an energy range from 10 to 40 keV. The results of the fiber light output and associated effects of an acrylate coating and the quantum dots application technique are discussed.
C1 [DeHaven, S. L.; Williams, P. A.; Burke, E. R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP DeHaven, SL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM stanton.l.dehaven@nasa.gov; phillip.a.williams@nasa.gov;
eric.r.burke@nasa.gov
NR 9
TC 0
Z9 0
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 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 110012
DI 10.1063/1.4940583
PG 8
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800137
ER
PT S
AU Johnson, WL
Kim, SA
White, GS
Herzberger, J
Peterson, KL
Heyliger, PR
AF Johnson, Ward L.
Kim, Sudook A.
White, Grady S.
Herzberger, Jaemi
Peterson, Kirsten L.
Heyliger, Paul R.
BE Chimenti, DE
Bond, LJ
TI Time-domain Analysis of Resonant Acoustic Nonlinearity Arising from
Cracks in Multilayer Ceramic Capacitors
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
ID QUALITY INSPECTION TOOL; DAMAGE; SPECTROSCOPY
AB Acoustic nonlinearity of cracked and uncracked multilayer ceramic capacitors (MLCCs) was characterized through time-domain analysis of resonant waveforms following tone-burst excitation. A phase-sensitive receiver was employed to measure the phase, relative to a reference sinusoid, of decaying oscillations of a resonant mode near 1 MHz that was excited through ferroelectric coupling within the barium-titanate-based ceramic of the MLCC. Amplitude dependence of the resonant frequency during decay of the oscillations was characterized through measurements of changes in the resonant phase versus time. Waveforms were analyzed by fitting the recorded RF amplitude versus time to a decaying exponential and inserting the parameters of this fit into a second function to fit the time-dependent phase, with amplitude dependence of the resonant frequency incorporated in the second function. The measurements and analyses were performed on unmounted type-1210 MLCCs before and after quenching in ice water from elevated temperatures. This thermal treatment generated surface-breaking cracks in a fraction of the specimens. Measurements of a nonlinear parameter B of the capacitors before quenching were used to set a range corresponding to plus and minus three standard deviations (+/- 3 sigma) relative to the mean of a Gaussian fit to the distribution of this parameter. 93% of the values of B determined for heat-treated MLCCs with cracks were outside of this +/- 3 sigma range of the as-received MLCCs, while only 10% of the values of B for heat-treated MLCCs without visible cracks were outside this range. These results indicate that time-domain nonlinear measurements with tone-burst excitation are a promising approach for rapid nondestructive detection of cracks that have no significant initial effect on the electrical characteristics of an MLCC but can evolve into conductive pathways during service and lead to electrical-device failure. They also illustrate the potential of this approach for nonlinear acoustic detection of structural flaws in other materials.
C1 [Johnson, Ward L.; Kim, Sudook A.; White, Grady S.] NIST, Appl Chem & Mat Div, 325 Broadway St, Boulder, CO 80305 USA.
[Herzberger, Jaemi] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA.
[Herzberger, Jaemi] NASA, Goddard Space Flight Ctr, Elect Parts & Packaging Program, Greenbelt, MD 20771 USA.
[Peterson, Kirsten L.; Heyliger, Paul R.] Colorado State Univ, Dept Civil & Environm Engn, Ft Collins, CO 80523 USA.
RP Johnson, WL (reprint author), NIST, Appl Chem & Mat Div, 325 Broadway St, Boulder, CO 80305 USA.
EM wjohnson@boulder.nist.gov
NR 14
TC 1
Z9 1
U1 4
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 060005
DI 10.1063/1.4940511
PG 10
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800065
ER
PT S
AU Leckey, CAC
Seebo, JP
Juarez, P
AF Leckey, Cara A. C.
Seebo, Jeffrey P.
Juarez, Peter
BE Chimenti, DE
Bond, LJ
TI Challenges of NDE Simulation Tool Validation, Optimization, and
Utilization for Composites
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
AB Rapid, realistic nondestructive evaluation (NDE) simulation tools can aid in inspection optimization and prediction of inspectability for advanced aerospace materials and designs. NDE simulation tools may someday aid in the design and certification of aerospace components; potentially shortening the time from material development to implementation by industry and government. Furthermore, ultrasound modeling and simulation are expected to play a significant future role in validating the capabilities and limitations of guided wave based structural health monitoring (SHM) systems. The current state-of-the-art in ultrasonic NDE/SHM simulation is still far from the goal of rapidly simulating damage detection techniques for large scale, complex geometry composite components/vehicles containing realistic damage types. Ongoing work at NASA Langley Research Center is focused on advanced ultrasonic simulation tool development. This paper discusses challenges of simulation tool validation, optimization, and utilization for composites. Ongoing simulation tool development work is described along with examples of simulation validation and optimization challenges that are more broadly applicable to all NDE simulation tools. The paper will also discuss examples of simulation tool utilization at NASA to develop new damage characterization methods for composites, and associated challenges in experimentally validating those methods.
C1 [Leckey, Cara A. C.; Juarez, Peter] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA.
[Seebo, Jeffrey P.] NASA, Langley Res Ctr, Analyt Mech Associates, Hampton, VA 23665 USA.
RP Leckey, CAC (reprint author), NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA.
EM cara.ac.leckey@nasa.gov
NR 4
TC 0
Z9 0
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 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 120011
DI 10.1063/1.4940596
PG 8
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800150
ER
PT S
AU Sammons, D
Winfree, WP
Burke, E
Ji, SW
AF Sammons, Daniel
Winfree, William P.
Burke, Eric
Ji, Shuiwang
BE Chimenti, DE
Bond, LJ
TI Segmenting Delaminations in Carbon Fiber Reinforced Polymer Composite CT
using Convolutional Neural Networks
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
ID IMAGES
AB Nondestructive evaluation (NDE) utilizes a variety of techniques to inspect various materials for defects without causing changes to the material. X-ray computed tomography (CT) produces large volumes of three dimensional image data. Using the task of identifying delaminations in carbon fiber reinforced polymer (CFRP) composite CT, this work shows that it is possible to automate the analysis of these large volumes of CT data using a machine learning model known as a convolutional neural network (CNN). Further, tests on simulated data sets show that with a robust set of experimental data, it may be possible to go beyond just identification and instead accurately characterize the size and shape of the delaminations with CNNs.
C1 [Sammons, Daniel; Winfree, William P.; Burke, Eric] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Sammons, Daniel; Ji, Shuiwang] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Sammons, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.; Sammons, D (reprint author), Old Dominion Univ, Norfolk, VA 23529 USA.
EM daniel.m.sammos@nasa.gov
NR 11
TC 0
Z9 0
U1 4
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 110014
DI 10.1063/1.4940585
PG 7
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800139
ER
PT S
AU Winfree, WP
Cramer, KE
Zalameda, JN
Howell, PA
AF Winfree, William P.
Cramer, K. Elliott
Zalameda, Joseph N.
Howell, Patricia A.
BE Chimenti, DE
Bond, LJ
TI Numerical Simulations of Thermographic Responses in Composites
SO 42ND ANNUAL REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE
EVALUATION: INCORPORATING THE 6TH EUROPEAN-AMERICAN WORKSHOP ON
RELIABILITY OF NDE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 42nd Annual Review of Progress in Quantitative Nondestructive Evaluation
(QNDE)
CY JUL 26-31, 2015
CL Minneapolis, MN
SP Ctr Nondestruct Evaluat, QNDE Programs
AB Numerical simulations of thermographic responses in composite materials have been useful for evaluating and optimizing thermographic analysis techniques. Numerical solutions are particularly beneficial for thermographic techniques, since the fabrication of specimens with realistic flaws is difficult. A quadrupole method for performing the simulations in two dimensions is presented. The results are compared to a finite element simulation of the same geometry. The technique is shown to be in good agreement with a finite element simulation of the same geometry, however, it requires about one hundredth of the computational time.
C1 [Winfree, William P.] NASA, Langley Res Ctr, MS 225, Hampton, VA 23681 USA.
[Cramer, K. Elliott; Zalameda, Joseph N.; Howell, Patricia A.] NASA, Langley Res Ctr, MS 231, Hampton, VA 23681 USA.
RP Winfree, WP (reprint author), NASA, Langley Res Ctr, MS 225, Hampton, VA 23681 USA.
EM william.p.winfree@nasa.gov
NR 19
TC 0
Z9 0
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 978-0-7354-1353-5
J9 AIP CONF PROC
PY 2016
VL 1706
AR 120012
DI 10.1063/1.4940597
PG 8
WC Physics, Applied
SC Physics
GA BE4LT
UT WOS:000371907800151
ER
PT S
AU Linthicum, KJ
Britch, SC
Anyamba, A
AF Linthicum, Kenneth J.
Britch, Seth C.
Anyamba, Assaf
BE Berenbaum, MR
TI Rift Valley Fever: An Emerging Mosquito-Borne Disease
SO ANNUAL REVIEW OF ENTOMOLOGY, VOL 61
SE Annual Review of Entomology
LA English
DT Review; Book Chapter
DE hemorrhagic disease; zoonosis; Aedes; Culex; disease forecasting;
environmental and climate linkages
ID NORTH-AMERICAN MOSQUITOS; SOUTH-AFRICA; DIPTERA-CULICIDAE; VECTOR
COMPETENCE; SAUDI-ARABIA; MECHANICAL TRANSMISSION; PHLEBOTOMUS-DUBOSCQI;
POTENTIAL VECTORS; CULEX-PIPIENS; EGYPT 1977-78
AB Rift Valley fever (RVF), an emerging mosquito-borne zoonotic infectious viral disease caused by the RVF virus (RVFV) (Bunyaviridae: Phlebovirus), presents significant threats to global public health and agriculture in Africa and the Middle East. RVFVis listed as a select agent with significant potential for international spread and use in bioterrorism. RVFVhas caused large, devastating periodic epizootics and epidemics in Africa over the past similar to 60 years, with severe economic and nutritional impacts on humans from illness and livestock loss. In the past 15 years alone, RVFV caused tens of thousands of human cases, hundreds of human deaths, and more than 100,000 domestic animal deaths. Cattle, sheep, goats, and camels are particularly susceptible to RVF and serve as amplifying hosts for the virus. This review highlights recent research on RVF, focusing on vectors and their ecology, transmission dynamics, and use of environmental and climate data to predict disease outbreaks. Important directions for future research are also discussed.
C1 [Linthicum, Kenneth J.; Britch, Seth C.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA.
[Anyamba, Assaf] NASA, Goddard Space Flight Ctr, GESTAR, USRA, Greenbelt, MD 20771 USA.
RP Linthicum, KJ (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA.
EM Kenneth.Linthicum@ars.usda.gov; Seth.Britch@ars.usda.gov;
Assaf.Anyamba@nasa.gov
NR 135
TC 8
Z9 9
U1 8
U2 19
PU ANNUAL REVIEWS
PI PALO ALTO
PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA
SN 0066-4170
BN 978-0-8243-0161-3
J9 ANNU REV ENTOMOL
JI Annu. Rev. Entomol.
PY 2016
VL 61
BP 395
EP +
DI 10.1146/annurev-ento-010715-023819
PG 32
WC Entomology
SC Entomology
GA BE5AB
UT WOS:000372413800022
PM 26982443
ER
PT J
AU Buermann, W
Beaulieu, C
Parida, B
Medvigy, D
Collatz, GJ
Sheffield, J
Sarmiento, JL
AF Buermann, Wolfgang
Beaulieu, Claudie
Parida, Bikash
Medvigy, David
Collatz, George J.
Sheffield, Justin
Sarmiento, Jorge L.
TI Climate-driven shifts in continental net primary production implicated
as a driver of a recent abrupt increase in the land carbon sink
SO BIOGEOSCIENCES
LA English
DT Article
ID ARCTIC OSCILLATION; CO2 FERTILIZATION; RECENT TRENDS; EL-NINO;
VARIABILITY; TEMPERATURE; VEGETATION; DIOXIDE; PRECIPITATION;
SENSITIVITY
AB The world's ocean and land ecosystems act as sinks for anthropogenic CO2, and over the last half century their combined sink strength grew steadily with increasing CO2 emissions. Recent analyses of the global carbon budget, however, have uncovered an abrupt, substantial (similar to 1 PgC yr(-1)) and sustained increase in the land sink in the late 1980s whose origin remains unclear. In the absence of this prominent shift in the land sink, increases in atmospheric CO2 concentrations since the late 1980s would have been similar to 30% larger than observed (or similar to 12 ppm above current levels). Global data analyses are limited in regards to attributing causes to changes in the land sink because different regions are likely responding to different drivers. Here, we address this challenge by using terrestrial biosphere models constrained by observations to determine if there is independent evidence for the abrupt strengthening of the land sink. We find that net primary production significantly increased in the late 1980s (more so than heterotrophic respiration), consistent with the inferred increase in the global land sink, and that large-scale climate anomalies are responsible for this shift. We identify two key regions in which climatic constraints on plant growth have eased: northern Eurasia experienced warming, and northern Africa received increased precipitation. Whether these changes in continental climates are connected is uncertain, but North Atlantic climate variability is important. Our findings suggest that improved understanding of climate variability in the North Atlantic may be essential for more credible projections of the land sink under climate change.
C1 [Buermann, Wolfgang] Univ Leeds, Sch Earth & Environm, Ins Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Beaulieu, Claudie] Univ Southampton, Natl Oceanog Ctr Southampton, Ocean & Earth Sci, Southampton SO14 3ZH, Hants, England.
[Parida, Bikash] Shiv Nadar Univ, Dept Civil Engn, Dadri 203207, UP, India.
[Medvigy, David; Sarmiento, Jorge L.] Princeton Univ, Atmospher & Ocean Sci Program, Princeton, NJ 08540 USA.
[Collatz, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08540 USA.
RP Buermann, W (reprint author), Univ Leeds, Sch Earth & Environm, Ins Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
EM w.buermann@leeds.ac.uk
RI collatz, george/D-5381-2012;
OI Sheffield, Justin/0000-0003-2400-0630
FU National Aeronautics and Space Administration Carbon Cycle Science
Program [NNX11AD45G]
FX We gratefully acknowledge support for this study from the National
Aeronautics and Space Administration Carbon Cycle Science Program (grant
NNX11AD45G).
NR 47
TC 0
Z9 0
U1 4
U2 17
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1726-4170
EI 1726-4189
J9 BIOGEOSCIENCES
JI Biogeosciences
PY 2016
VL 13
IS 5
BP 1597
EP 1607
DI 10.5194/bg-13-1597-2016
PG 11
WC Ecology; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DG4ZU
UT WOS:000372082500014
ER
PT J
AU Carmichael, MJ
Lunt, DJ
Huber, M
Heinemann, M
Kiehl, J
LeGrande, A
Loptson, CA
Roberts, CD
Sagoo, N
Shields, C
Valdes, PJ
Winguth, A
Winguth, C
Pancost, RD
AF Carmichael, Matthew J.
Lunt, Daniel J.
Huber, Matthew
Heinemann, Malte
Kiehl, Jeffrey
LeGrande, Allegra
Loptson, Claire A.
Roberts, Chris D.
Sagoo, Navjit
Shields, Christine
Valdes, Paul J.
Winguth, Arne
Winguth, Cornelia
Pancost, Richard D.
TI A model-model and data-model comparison for the early Eocene
hydrological cycle
SO CLIMATE OF THE PAST
LA English
DT Article
ID PALAEOCENE/EOCENE THERMAL MAXIMUM; PACIFIC CONVERGENCE ZONE; COUPLED
CLIMATE MODEL; CLAY-MINERAL EVIDENCE; LATE PALEOCENE; CARBON-CYCLE;
NEW-ZEALAND; TROPICAL PRECIPITATION; ATMOSPHERIC CO2; OXYGEN-ISOTOPE
AB A range of proxy observations have recently provided constraints on how Earth's hydrological cycle responded to early Eocene climatic changes. However, comparisons of proxy data to general circulation model (GCM) simulated hydrology are limited and inter-model variability remains poorly characterised. In this work, we undertake an intercomparison of GCM-derived precipitation and P-E distributions within the extended EoMIP ensemble ( Eocene Modelling Intercomparison Project; Lunt et al., 2012), which includes previously published early Eocene simulations performed using five GCMs differing in boundary conditions, model structure, and precipitation-relevant parameterisation schemes.
We show that an intensified hydrological cycle, manifested in enhanced global precipitation and evaporation rates, is simulated for all Eocene simulations relative to the preindustrial conditions. This is primarily due to elevated atmospheric paleo-CO2, resulting in elevated temperatures, although the effects of differences in paleogeography and ice sheets are also important in some models. For a given CO2 level, globally averaged precipitation rates vary widely between models, largely arising from different simulated surface air temperatures. Models with a similar global sensitivity of precipitation rate to temperature (dP/dT) display different regional precipitation responses for a given temperature change. Regions that are particularly sensitive to model choice include the South Pacific, tropical Africa, and the Peri-Tethys, which may represent targets for future proxy acquisition.
A comparison of early and middle Eocene leaf-fossilderived precipitation estimates with the GCM output illustrates that GCMs generally underestimate precipitation rates at high latitudes, although a possible seasonal bias of the proxies cannot be excluded. Models which warm these regions, either via elevated CO2 or by varying poorly constrained model parameter values, are most successful in simulating a match with geologic data. Further data from low-latitude regions and better constraints on early Eocene CO2 are now required to discriminate between these model simulations given the large error bars on paleoprecipitation estimates. Given the clear differences between simulated precipitation distributions within the ensemble, our results suggest that paleohydrological data offer an independent means by which to evaluate model skill for warm climates.
C1 [Carmichael, Matthew J.; Lunt, Daniel J.; Loptson, Claire A.; Sagoo, Navjit; Valdes, Paul J.] Univ Bristol, Sch Geog Sci, BRIDGE, Bristol, Avon, England.
[Carmichael, Matthew J.; Lunt, Daniel J.; Loptson, Claire A.; Sagoo, Navjit; Valdes, Paul J.; Pancost, Richard D.] Univ Bristol, Cabot Inst, Bristol, Avon, England.
[Carmichael, Matthew J.; Pancost, Richard D.] Univ Bristol, Sch Chem, Organ Geochem Unit, Bristol BS8 1TS, Avon, England.
[Huber, Matthew] Univ New Hampshire, Dept Earth Sci, Climate Dynam Predict Lab, Durham, NH 03824 USA.
[Heinemann, Malte] Univ Kiel, Inst Geosci, Kiel, Germany.
[Kiehl, Jeffrey] UCAR NCAR, Climate & Global Dynam Lab, Boulder, CO USA.
[LeGrande, Allegra] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Roberts, Chris D.] Met Off, Exeter, Devon, England.
[Winguth, Arne; Winguth, Cornelia] Univ Texas Arlington, Dept Earth & Environm Sci, Climate Res Grp, Arlington, TX USA.
[Sagoo, Navjit] Yale Univ, Dept Geol & Geophys, New Haven, CT USA.
RP Carmichael, MJ (reprint author), Univ Bristol, Sch Geog Sci, BRIDGE, Bristol, Avon, England.; Carmichael, MJ (reprint author), Univ Bristol, Cabot Inst, Bristol, Avon, England.; Carmichael, MJ (reprint author), Univ Bristol, Sch Chem, Organ Geochem Unit, Bristol BS8 1TS, Avon, England.
EM matt.carmichael@bristol.ac.uk
RI Huber, Matthew/A-7677-2008; Valdes, Paul/C-4129-2013
OI Huber, Matthew/0000-0002-2771-9977;
FU NERC grant Cretaceous-Paleocene-Eocene: Exploring Climate and Climate
Sensitivity [NE/K014757/1]; Royal Society
FX Daniel J. Lunt acknowledges support through the NERC grant
Cretaceous-Paleocene-Eocene: Exploring Climate and Climate Sensitivity
(NE/K014757/1). Richard D. Pan-cost acknowledges the Royal Society for a
Wolfson Research Merit Award. Finally, we thank two anonymous reviewers
for their constructive comments, which improved the quality of this
manuscript.
NR 170
TC 3
Z9 3
U1 6
U2 18
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1814-9324
EI 1814-9332
J9 CLIM PAST
JI Clim. Past.
PY 2016
VL 12
IS 2
BP 455
EP 481
DI 10.5194/cp-12-455-2016
PG 27
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences
SC Geology; Meteorology & Atmospheric Sciences
GA DF8RH
UT WOS:000371625400016
ER
PT J
AU Lyons, C
Eckert, G
Stoner, AW
AF Lyons, Courtney
Eckert, Ginny
Stoner, Allan W.
TI INFLUENCE OF TEMPERATURE AND CONGENER PRESENCE ON HABITAT PREFERENCE AND
FISH PREDATION IN BLUE (PARALITHODES PLATYPUS BRANDT, 1850) AND RED (P.
CAMTSCHATICUS TILESIUS, 1815) KING CRABS (ANOMURA: LITHODIDAE)
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE Alaska; climate change; fish predation; multi-species interactions
ID CLIMATE-CHANGE; JUVENILE RED; BEHAVIORAL PLASTICITY;
FUNCTIONAL-RESPONSE; FORAGING SUCCESS; STOCK ASSESSMENT;
RUTILUS-RUTILUS; CANNIBALISM; COMPLEXITY; SURVIVAL
AB Rebuilding fisheries is a difficult process and many stocks that are declared overfished fail to recover even in the absence of fishing pressure. The Pribilof Islands stock of the blue king crab (Paralithodes platypus Brandt, 1850) in Alaska, USA is one of these recovery failures. To explore how environmental and ecological factors might interact to suppress this stock, we conducted a suite of laboratory experiments to assess the effects of temperature changes and the presence of red king crab (Paralithodes camtschaticus Tilesius, 1815) on blue king crab habitat preference and fish predation survival. Age-0 blue king crabs exhibited plasticity in habitat preference mediated by changes in water temperature, as well as the presence and density of juvenile red king crabs. While blue king crabs are often associated with shell hash habitat, increases in water temperature, as well as the presence of red king crab at high densities, caused blue king crab juveniles to shift into habitats with an algal mimic present, a habitat type shown to reduce the predation efficacy of red king crabs. In contrast, red king crabs exhibited fewer changes in habitat preference with changes in water temperature and the presence of a congener. Blue king crabs are therefore behaviorally plastic, switching from strategies of predator avoidance when predator encounter rates are likely low, to predator deterrence strategies when encounter rates are higher. Fish predation trials further support the idea that blue king crabs are more focused on predator avoidance than are red king crabs. In fish predation trials run separately for the two crab species, blue king crabs had higher survival (60%) than red king crabs (33%) when exposed to fish predators. Our results indicate that age -0 blue king crabs can be less vulnerable to fish predation than red king crabs, but future research should assess how fish predation rates change when presented with higher densities of red and blue king crab in mixed assemblages as the observed habitat shifts could affect predation survival.
C1 [Lyons, Courtney; Eckert, Ginny] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Pt Lena Loop Rd, Juneau, AK USA.
[Stoner, Allan W.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 20305 Marine Sci Dr, Newport, OR 97365 USA.
RP Lyons, C (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Pt Lena Loop Rd, Juneau, AK USA.
EM courtney.lyons@gmail.com
FU National Science Foundation Marine Ecosystem Sustainability in the
Arctic and Subarctic (MESAS) IGERT program [DGE-0801720]; Rasmuson
Fisheries Research Center; National Sea Grant Aquaculture
FX Thanks are due to Michelle Ottmar, Scott Haines, and Courtney Danly for
help conducting experiments and maintaining the animals. We also thank
Ben Daly for advice on experiments and Franz Mueter for advice on
analysis. Funding was provided by the National Sea Grant Aquaculture,
National Science Foundation Marine Ecosystem Sustainability in the
Arctic and Subarctic (MESAS) IGERT program (No. DGE-0801720), and the
Rasmuson Fisheries Research Center. Research was conducted under the UAF
IACUC permit 280889.
NR 59
TC 0
Z9 0
U1 3
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0278-0372
EI 1937-240X
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD JAN
PY 2016
VL 36
IS 1
BP 12
EP 22
DI 10.1163/1937240X-00002391
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DG0KJ
UT WOS:000371753400002
ER
PT J
AU Shaygan, M
Davami, K
Jin, B
Gemming, T
Lee, JS
Meyyappan, M
AF Shaygan, Mehrdad
Davami, Keivan
Jin, Bo
Gemming, Thomas
Lee, Jeong-Soo
Meyyappan, M.
TI Highly sensitive photodetectors using ZnTe/ZnO core/shell nanowire field
effect transistors with a tunable core/shell ratio
SO JOURNAL OF MATERIALS CHEMISTRY C
LA English
DT Article
ID CORE-SHELL NANOWIRES; PHOTOVOLTAIC APPLICATIONS; IN-SITU; ZNO;
HETEROSTRUCTURES; GROWTH
AB The fabrication and characterization of a field effect transistor using a radial core/shell structure based on ZnTe nanowires is reported here. The electronic and photoconductive performance of the devices is successfully controlled by tuning the shell to core ratios in the integrated devices. The ZnO shell around the ZnTe nanowire has a significant effect on the optical properties of the transistor, and the photo-to-dark current ratio, responsivity and photoconductive gain are greatly enhanced to 199, 196 and 8.12 x 10(4)% respectively for the 17.5% shell/core ratio. The ability to control the core/shell ratio presented here is promising in device design for optoelectronic applications for covering a wide range of wavelengths.
C1 [Shaygan, Mehrdad] AMO GmbH, Adv Microelect Ctr Aachen AMICA, Otto Blumenthal Str 25, D-52074 Aachen, Germany.
[Davami, Keivan] Univ Penn, Dept Mech Engn & Appl Mech, Philadelphia, PA 19104 USA.
[Davami, Keivan] Widener Univ, Dept Mech Engn, One Univ Pl, Chester, PA 19013 USA.
[Jin, Bo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang, South Korea.
[Gemming, Thomas] IFW Dresden, POB 270116, D-01171 Dresden, Germany.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Shaygan, M (reprint author), AMO GmbH, Adv Microelect Ctr Aachen AMICA, Otto Blumenthal Str 25, D-52074 Aachen, Germany.
EM shaygan@amo.de
NR 38
TC 2
Z9 2
U1 6
U2 26
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2050-7526
EI 2050-7534
J9 J MATER CHEM C
JI J. Mater. Chem. C
PY 2016
VL 4
IS 10
BP 2040
EP 2046
DI 10.1039/c5tc03999a
PG 7
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA DF9HJ
UT WOS:000371671400015
ER
PT J
AU Kumar-Krishnan, S
Chakaravarthy, S
Hernandez-Rangel, A
Prokhorov, E
Luna-Barcenas, G
Esparza, R
Meyyappan, M
AF Kumar-Krishnan, Siva
Chakaravarthy, S.
Hernandez-Rangel, A.
Prokhorov, E.
Luna-Barcenas, G.
Esparza, Rodrigo
Meyyappan, M.
TI Chitosan supported silver nanowires as a platform for direct
electrochemistry and highly sensitive electrochemical glucose biosensing
(vol 6, pg 20102, 2016)
SO RSC ADVANCES
LA English
DT Correction
C1 [Kumar-Krishnan, Siva; Hernandez-Rangel, A.; Prokhorov, E.; Luna-Barcenas, G.] Cinvestav Queretaro, Queretaro 76230, Qro, Mexico.
[Kumar-Krishnan, Siva; Esparza, Rodrigo] Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Blvd Juriquilla 3001, Santiago De Queretaro 76230, Qro, Mexico.
[Chakaravarthy, S.] CINVESTAV IPN, Programa Doctorado Nanociencias & Nanotecnol, Mexico City 07360, DF, Mexico.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kumar-Krishnan, S; Luna-Barcenas, G (reprint author), Cinvestav Queretaro, Queretaro 76230, Qro, Mexico.; Kumar-Krishnan, S (reprint author), Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Blvd Juriquilla 3001, Santiago De Queretaro 76230, Qro, Mexico.
EM skumar@fata.unam.mx; glunascf@yahoo.com
NR 1
TC 0
Z9 0
U1 7
U2 11
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2046-2069
J9 RSC ADV
JI RSC Adv.
PY 2016
VL 6
IS 27
BP 22950
EP 22950
DI 10.1039/c6ra90021f
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA DF9XQ
UT WOS:000371716300083
ER
PT S
AU Stam, C
Behar, A
Cooper, M
AF Stam, Christina
Behar, Alberto
Cooper, Moogega
BE Micic, M
TI Sampling of Microbiological Samples
SO SAMPLE PREPARATION TECHNIQUES FOR SOIL, PLANT, AND ANIMAL SAMPLES
SE Springer Protocols Handbooks
LA English
DT Article; Book Chapter
DE Air; Aseptic; Contamination; Filtration; Feeds; HVB; RODAC; Surfaces;
Swabs; Vacuum-sampling; Water; Wipes
ID DRY DOG FOOD; UNITED-STATES; ENVIRONMENTAL SURFACES; NONPOROUS SURFACES;
BACILLUS SPORES; COLLECTION; INFECTIONS; RECOVERY; CANADA; SWABS
AB Sampling of microorganisms from the environment presents a unique set of challenges. The various matrices in which microorganisms can survive and persist, along with the diversity in the communities that make up these environments are complex. Several types of methods exist for the detection and isolation of microbes from the environment. These methods include a variety of surface and air sampling techniques, as well as additional methodology specific to water and food samples.
C1 [Stam, Christina; Behar, Alberto] US FDA, 6502 S Archer Rd, Bedford Pk, IL 60501 USA.
[Stam, Christina; Behar, Alberto] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
[Cooper, Moogega] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
RP Cooper, M (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM Christina.stam@fda.hhs.gov; alberto.behar@jpl.nasa.gov;
moogega.cooper@jpl.nasa.gov
NR 35
TC 0
Z9 0
U1 2
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1949-2448
BN 978-1-4939-3185-9; 978-1-4939-3184-2
J9 SPRINGER PROTOC HAND
PY 2016
BP 25
EP 39
DI 10.1007/978-1-4939-3185-9_3
D2 10.1007/978-1-4939-3185-9
PG 15
WC Plant Sciences
SC Plant Sciences
GA BE4EL
UT WOS:000371627100005
ER
PT S
AU Cooper, M
Stam, C
AF Cooper, Moogega
Stam, Christina
BE Micic, M
TI Nucleic Acid Purification from Soil and Environmental Sources
SO SAMPLE PREPARATION TECHNIQUES FOR SOIL, PLANT, AND ANIMAL SAMPLES
SE Springer Protocols Handbooks
LA English
DT Article; Book Chapter
DE DNA; Soil; Purification
ID RIBOSOMAL-RNA; MICROBIAL DIVERSITY; DIRECT EXTRACTION; DNA EXTRACTION;
BACTERIAL-DNA; HUMIC ACIDS; PCR; SAMPLES; MICROORGANISMS; SEDIMENTS
AB The extraction of nucleic acids from soil and environmental samples allows scientists the opportunity to discern the microbial community irrespective of viability and cultivability. General nucleic acid extraction and purification approaches are discussed as well as their limitations. Soil type and humic acid content are among many factors that can affect the processing approach. The environmental sample collection, extraction, and purification protocol developed for a low-population density cleanroom environment is discussed as a specific example of environmental sample processing. This practical application of DNA purification techniques were used to assess microbial diversity and abundance in spacecraft assembly cleanrooms.
C1 [Cooper, Moogega] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
[Stam, Christina] US FDA, 6502 S Archer Rd, Bedford Pk, IL 60501 USA.
RP Cooper, M (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM moogega.cooper@jpl.nasa.gov; Christina.stam@fda.hhs.gov
NR 37
TC 0
Z9 0
U1 3
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1949-2448
BN 978-1-4939-3185-9; 978-1-4939-3184-2
J9 SPRINGER PROTOC HAND
PY 2016
BP 307
EP 314
DI 10.1007/978-1-4939-3185-9_21
D2 10.1007/978-1-4939-3185-9
PG 8
WC Plant Sciences
SC Plant Sciences
GA BE4EL
UT WOS:000371627100023
ER
PT J
AU Khosrawi, F
Urban, J
Lossow, S
Stiller, G
Weigel, K
Braesicke, P
Pitts, MC
Rozanov, A
Burrows, JP
Murtagh, D
AF Khosrawi, F.
Urban, J.
Lossow, S.
Stiller, G.
Weigel, K.
Braesicke, P.
Pitts, M. C.
Rozanov, A.
Burrows, J. P.
Murtagh, D.
TI Sensitivity of polar stratospheric cloud formation to changes in water
vapour and temperature
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID NITRIC-ACID TRIHYDRATE; HALOGEN OCCULTATION EXPERIMENT; SCIAMACHY LIMB
MEASUREMENTS; ARCTIC WINTER 2010/2011; OZONE LOSS; TROPICAL TROPOPAUSE;
NAT FORMATION; TRACE GASES; FROST POINT; MIPAS
AB More than a decade ago it was suggested that a cooling of stratospheric temperatures by 1 K or an increase of 1 ppmv of stratospheric water vapour could promote denitrification, the permanent removal of nitrogen species from the stratosphere by solid polar stratospheric cloud (PSC) particles. In fact, during the two Arctic winters 2009/10 and 2010/11 the strongest denitrification in the recent decade was observed. Sensitivity studies along air parcel trajectories are performed to test how a future stratospheric water vapour (H2O) increase of 1 ppmv or a temperature decrease of 1K would affect PSC formation. We perform our study based on measurements made during the Arctic winter 2010/11. Air parcel trajectories were calculated 6 days backward in time based on PSCs detected by CALIPSO (Cloud Aerosol Lidar and Infrared Pathfinder satellite observations). The sensitivity study was performed on single trajectories as well as on a trajectory ensemble. The sensitivity study shows a clear prolongation of the potential for PSC formation and PSC existence when the temperature in the stratosphere is decreased by 1K and water vapour is increased by 1 ppmv. Based on 15 years of satellite measurements (20002014) from UARS/HALOE, Envisat/MIPAS, Odin/SMR, Aura/MLS, Envisat/SCIAMACHY and SCISAT/ACE-FTS it is further investigated if there is a decrease in temperature and/or increase of water vapour (H2O) observed in the polar regions similar to that observed at midlatitudes and in the tropics. Performing linear regression analyses we derive from the Envisat/MIPAS (2002-2012) and Aura/MLS (2004-2014) observations predominantly positive changes in the potential temperature range 350 to 1000 K. The linear changes in water vapour derived from Envisat/MIPAS observations are largely insignificant, while those from Aura/MLS are mostly significant. For the temperature neither of the two instruments indicate any significant changes. Given the strong inter-annual variation observed in water vapour and particular temperature the severe denitrification observed in 2010/11 cannot be directly related to any changes in water vapour and temperature since the millennium. However, the observations indicate a clear correlation between cold winters and enhanced water vapour mixing ratios. This indicates a connection between dynamical and radiative processes that govern water vapour and temperature in the Arctic lower stratosphere.
C1 [Khosrawi, F.] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.
[Urban, J.; Murtagh, D.] Chalmers, Dept Earth & Space Sci, S-41296 Gothenburg, Sweden.
[Khosrawi, F.; Lossow, S.; Stiller, G.; Braesicke, P.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
[Weigel, K.; Rozanov, A.; Burrows, J. P.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
[Pitts, M. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Khosrawi, F (reprint author), Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.; Khosrawi, F (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
EM farahnaz.khosrawi@kit.edu
RI Murtagh, Donal/F-8694-2011; Braesicke, Peter/D-8330-2016; Burrows,
John/B-6199-2014
OI Murtagh, Donal/0000-0003-1539-3559; Braesicke,
Peter/0000-0003-1423-0619; Burrows, John/0000-0002-6821-5580
FU Swedish National Space Board (SNSB); Canadian Space Agency (SCA);
National Technology Agency of Finland (Tekes); Centre National d'Etudes
Spatiales (CNES) in France; CSA; National Sciences and Engineering
Research Council of Canada (NSERC); FP7 project RECONCILE
[RECONCILE-226365-FP7-ENV-2008-1]; German Research Foundation (DFG)
within the project SHARP [STI 210/9-2]; Deutsche Forschungsgemeinschaft;
Open Access Publishing Fund of Karlsruhe Institute of Technology
FX We are grateful to the European Space Agency (ESA) for providing
Odin/SMR data. Odin is a Swedish-led satellite project jointly funded by
the Swedish National Space Board (SNSB), the Canadian Space Agency
(SCA), the National Technology Agency of Finland (Tekes) and the Centre
National d'Etudes Spatiales (CNES) in France. SCISAT/ACE is a Canadian
led mission mainly supported by the CSA and National Sciences and
Engineering Research Council of Canada (NSERC). Provision of MIPAS
level-1b data by ESA is gratefully acknowledged. We also would like to
thank the MLS team for providing their data. MLS data were obtained from
the NASA Goddard Earth Sciences Data and Information Center. The
SCIAMACHY limb water vapour data V3.01 are a result of the DFG Research
Unit "Stratospheric Change and its role for Climate Prediction (SHARP)"
and the ESA Project SPIN (ESA SPARC Initiative) and were partly
calculated using resources of the German HLRN (High-Performance Computer
Center North). We also would like to thank M. Hervig for providing a
program to calculate the NAT existence temperature. We gratefully
acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of
the HYSPLIT READY website (http://ready.arl.noaa.gov/HYSPLIT.php). We
further acknowledge the helpful comments from the two anonymous
referees. This study was performed in the frame of the FP7 project
RECONCILE (Grant number: RECONCILE-226365-FP7-ENV-2008-1). We are also
grateful to Swedish National Space Board (SNSB) for funding F. Khosrawi
(2012-2013) and the German Research Foundation (DFG) for funding S
Lossow within the project SHARP under contract STI 210/9-2. We
acknowledge support by Deutsche Forschungsgemeinschaft and Open Access
Publishing Fund of Karlsruhe Institute of Technology.
NR 84
TC 1
Z9 1
U1 2
U2 9
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 1
BP 101
EP 121
DI 10.5194/acp-16-101-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YG
UT WOS:000371283900007
ER
PT J
AU Jeong, U
Kim, J
Ahn, C
Torres, O
Liu, X
Bhartia, PK
Spurr, RJD
Haffner, D
Chance, K
Holben, BN
AF Jeong, U.
Kim, J.
Ahn, C.
Torres, O.
Liu, X.
Bhartia, P. K.
Spurr, R. J. D.
Haffner, D.
Chance, K.
Holben, B. N.
TI An optimal-estimation-based aerosol retrieval algorithm using OMI
near-UV observations
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID OZONE-MONITORING INSTRUMENT; SKY RADIANCE MEASUREMENTS;
OPTICAL-PROPERTIES; PARTICLE NONSPHERICITY; TROPOSPHERIC AEROSOLS;
SPECTRAL REFLECTANCE; SATELLITE; AERONET; ABSORPTION; MODELS
AB An optimal-estimation(OE)-based aerosol retrieval algorithm using the OMI (Ozone Monitoring Instrument) near-ultraviolet observation was developed in this study. The OE-based algorithm has the merit of providing useful estimates of errors simultaneously with the inversion products. Furthermore, instead of using the traditional look-up tables for inversion, it performs online radiative transfer calculations with the VLIDORT (linearized pseudo-spherical vector discrete ordinate radiative transfer code) to eliminate interpolation errors and improve stability. The measurements and inversion products of the Distributed Regional Aerosol Gridded Observation Network campaign in northeast Asia (DRAGON NE-Asia 2012) were used to validate the retrieved aerosol optical thickness (AOT) and single scattering albedo (SSA). The retrieved AOT and SSA at 388 nm have a correlation with the Aerosol Robotic Network (AERONET) products that is comparable to or better than the correlation with the operational product during the campaign. The OE-based estimated error represented the variance of actual biases of AOT at 388 nm between the retrieval and AERONET measurements better than the operational error estimates. The forward model parameter errors were analyzed separately for both AOT and SSA retrievals. The surface reflectance at 388 nm, the imaginary part of the refractive index at 354 nm, and the number fine-mode fraction (FMF) were found to be the most important parameters affecting the retrieval accuracy of AOT, while FMF was the most important parameter for the SSA retrieval. The additional information provided with the retrievals, including the estimated error and degrees of freedom, is expected to be valuable for relevant studies. Detailed advantages of using the OE method were described and discussed in this paper.
C1 [Jeong, U.; Kim, J.] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Ahn, C.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Torres, O.; Bhartia, P. K.; Haffner, D.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Spurr, R. J. D.] RT Solut Inc, 9 Channing St, Cambridge, MA USA.
RP Kim, J (reprint author), Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
EM jkim2@yonsei.ac.kr
RI Liu, Xiong/P-7186-2014
OI Liu, Xiong/0000-0003-2939-574X
FU GEMS program of the Ministry of Environment, Korea; Eco Innovation
Program of KEITI [2012000160002]
FX This research was supported by the GEMS program of the Ministry of
Environment, Korea, and the Eco Innovation Program of KEITI
(2012000160002). The authors also acknowledge the KNMI and NASA/GSFC for
providing OMI and AERONET data, respectively. Authors also acknowledge
all the P. I.s and staff for the contribution to the DRAGON-NE Asia
campaign.
NR 59
TC 2
Z9 2
U1 0
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 1
BP 177
EP 193
DI 10.5194/acp-16-177-2016
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YG
UT WOS:000371283900012
ER
PT J
AU Padulles, R
Cardellach, E
Juarez, MD
Tomas, S
Turk, FJ
Oliveras, S
Ao, CO
Rius, A
AF Padulles, R.
Cardellach, E.
Juarez, M. de la Torre
Tomas, S.
Turk, F. J.
Oliveras, S.
Ao, C. O.
Rius, A.
TI Atmospheric polarimetric effects on GNSS radio occultations: the
ROHP-PAZ field campaign
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID GLOBAL POSITIONING SYSTEM; ICE PARTICLES; RADAR REFLECTIVITY; EARTHS
ATMOSPHERE; WATER-CONTENT; INVERSION; SHAPE
AB This study describes the first experimental observations showing that hydrometeors induce polarimetric signatures in global navigation satellite system (GNSS) signals. This evidence is relevant to the PAZ low Earth orbiter, which will test the concept and applications of polarimetric GNSS radio occultation (RO) (i.e. ROs obtained with a dual-polarization antenna). A ground field campaign was carried out in preparation for PAZ to verify the theoretical sensitivity studies on this concept (Cardellach et al., 2015). The main aim of the campaign is to identify and understand the factors that might affect the polarimetric GNSS observables. Studied for the first time, GNSS signals measured with two polarimetric antennas (H, horizontal, and V, vertical) are shown to discriminate between heavy rain events by comparing the measured phase difference between the H and V phase delays (18) in different weather scenarios. The measured phase difference indicates higher dispersion under rain conditions. When individual events are examined, significant increases in 18 occur when the radio signals cross rain cells. Moreover, the amplitude of such a signal is much higher than the theoretical prediction for precipitation; thus, other sources of polarimetric signatures have been explored and identified. Modelling of other hydrometeors, such as melting particles and ice crystals, have been proposed to explain the obtained measurements, with good agreement in more than 90% of the cases.
C1 [Padulles, R.; Cardellach, E.; Tomas, S.; Oliveras, S.; Rius, A.] Inst Ciencies Espai ICE CSIC IEEC, Barcelona, Spain.
[Juarez, M. de la Torre; Turk, F. J.; Ao, C. O.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Padulles, R (reprint author), Inst Ciencies Espai ICE CSIC IEEC, Barcelona, Spain.
EM padulles@ice.cat
OI Padulles, Ramon/0000-0003-2058-3779; Cardellach,
Estel/0000-0001-8908-0972
FU Spanish FPI program; Spanish Ramon y Cajal programme; NASA ROSES
[NNH14ZDA001N-ESUSPI, NNH10ZDA001N-GEOIM, NNH11ZDA001N-ESI]; Universitat
Politecnica de Catalunya [AYA2011-29183-C02-01]; European ERDF/FEDER
programme; [ACI2010-1089]; [AYA2011-29183-C02-02]
FX This study was conducted under the Spanish ACI2010-1089 and
AYA2011-29183-C02-02 grant, with contributions from EUMETSAT's ROM SAF
CDOP2. R. Padulles is supported by the Spanish FPI program and he also
received three JPL Vistor Student Researcher Program invitations. E.
Cardellach is supported by the Spanish Ramon y Cajal programme. Work
contributed by C. O. Ao, M. de la Torre Juarez, and F. J. Turk was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. Funding support from NASA ROSES Grants
NNH14ZDA001N-ESUSPI, NNH10ZDA001N-GEOIM, and NNH11ZDA001N-ESI is
gratefully acknowledged. A relevant contribution to the logistics and
implementation of the experimental site was made by Adriano Camps' group
at the Remote Sensing Lab, department of Teoria del Senyal i
Comunicacions, Universitat Politecnica de Catalunya, under grant
AYA2011-29183-C02-01. Some of these grants are partially funded by the
European ERDF/FEDER programme.
NR 32
TC 3
Z9 3
U1 2
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 2
BP 635
EP 649
DI 10.5194/acp-16-635-2016
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YH
UT WOS:000371284000012
ER
PT J
AU Zamora, LM
Kahn, RA
Cubison, MJ
Diskin, GS
Jimenez, JL
Kondo, Y
McFarquhar, GM
Nenes, A
Thornhill, KL
Wisthaler, A
Zelenyuk, A
Ziemba, LD
AF Zamora, L. M.
Kahn, R. A.
Cubison, M. J.
Diskin, G. S.
Jimenez, J. L.
Kondo, Y.
McFarquhar, G. M.
Nenes, A.
Thornhill, K. L.
Wisthaler, A.
Zelenyuk, A.
Ziemba, L. D.
TI Aircraft-measured indirect cloud effects from biomass burning smoke in
the Arctic and subarctic
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AEROSOL-SIZE DISTRIBUTIONS; IN-SITU CHARACTERIZATION; MIXED-PHASE
CLOUDS; CONDENSATION NUCLEI; SPLAT II; PERFORMANCE-CHARACTERISTICS;
STRATIFORM CLOUDS; MASS-SPECTROMETER; FIELD CAMPAIGN; BOREAL FORESTS
AB The incidence of wildfires in the Arctic and subarctic is increasing; in boreal North America, for example, the burned area is expected to increase by 200-300% over the next 50-100 years, which previous studies suggest could have a large effect on cloud microphysics, lifetime, albedo, and precipitation. However, the interactions between smoke particles and clouds remain poorly quantified due to confounding meteorological influences and remote sensing limitations. Here, we use data from several aircraft campaigns in the Arctic and subarctic to explore cloud microphysics in liquid-phase clouds influenced by biomass burning. Median cloud droplet radii in smoky clouds were similar to 40-60% smaller than in background clouds. Based on the relationship between cloud droplet number (N-liq ) and various biomass burning tracers (BBt ) across the multi-campaign data set, we calculated the magnitude of subarctic and Arctic smoke aerosol-cloud interactions (ACIs, where ACI = (1/3 x dln. N-liq/dln(BBt) to be similar to 0.16 out of a maximum possible value of 0.33 that would be obtained if all aerosols were to nucleate cloud droplets. Interestingly, in a separate subarctic case study with low liquid water content
C1 [Zamora, L. M.; Kahn, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Zamora, L. M.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Cubison, M. J.; Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Diskin, G. S.; Thornhill, K. L.; Ziemba, L. D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kondo, Y.] Natl Inst Polar Res, Tokyo, Japan.
[McFarquhar, G. M.] Univ Illinois, Urbana, IL USA.
[Nenes, A.] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Nenes, A.] Fdn Res & Technol Hellas, Patras, Greece.
[Nenes, A.] Natl Observ Athens, Athens, Greece.
[Wisthaler, A.] Univ Oslo, Dept Chem, Oslo, Norway.
[Wisthaler, A.] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Zelenyuk, A.] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Zamora, LM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.; Zamora, LM (reprint author), Oak Ridge Associated Univ, Oak Ridge, TN USA.
EM lauren.m.zamora@nasa.gov
RI Jimenez, Jose/A-5294-2008;
OI Jimenez, Jose/0000-0001-6203-1847; McFarquhar, Greg/0000-0003-0950-0135;
Zamora, Lauren/0000-0002-0878-4378
FU U.S. Department of Energy, Office of Science, Office of Biological and
Environmental Research, Climate and Environmental Sciences Division;
Austrian Federal Ministry for Transport, Innovation and Technology
(bmvit) through the Austrian Space Applications Programme (ASAP) of the
Austrian Research Promotion Agency (FFG); NASA Postdoctoral Program at
Goddard Space Flight Center; NASA [NNX12AC03G, NNX15AH33A]
FX The authors would like to thank A. Aknan, B. Anderson, E. Apel, G. Chen,
M. Couture, T. Garrett, K. B. Huebert, A. Khain, A. Korolev, T. Lathem,
P. Lawson, R. Leaitch, J. Limbacher, J. Nelson, M. Pinsky, W. Ridgeway,
A. Rangno, S. Williams, S. Woods, and Y. Yang for data and/or advice or
help with various aspects of this project, and all others who were
involved in collecting and funding the collection of the data sets we
have used. We acknowledge the Atmospheric Radiation Measurement (ARM)
Program sponsored by the U.S. Department of Energy, Office of Science,
Office of Biological and Environmental Research, Climate and
Environmental Sciences Division for providing the ISDAC data set. The
authors also gratefully acknowledge the NOAA Air Resources Laboratory
(ARL) for the provision of the HYSPLIT transport and dispersion model
and/or READY website (http://www.ready.noaa.gov) used in this
publication. Plots were made with Ocean Data View (Schlitzer, R., Ocean
Data View, http://odv.awi.de, 2015) and R (R Core Team, 2013).
CH3CN measurements were supported by the Austrian Federal
Ministry for Transport, Innovation and Technology (bmvit) through the
Austrian Space Applications Programme (ASAP) of the Austrian Research
Promotion Agency (FFG). T. Mikoviny is acknowledged for his support with
the CH3CN data acquisition and analysis. LMZ's funding for
this study was provided by an appointment to the NASA Postdoctoral
Program at Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. M. J. Cubison and
J. L. Jimenez were supported by NASA NNX12AC03G and NNX15AH33A.
NR 127
TC 2
Z9 2
U1 4
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 2
BP 715
EP 738
DI 10.5194/acp-16-715-2016
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YH
UT WOS:000371284000017
ER
PT J
AU Beyersdorf, AJ
Ziemba, LD
Chen, G
Corr, CA
Crawford, JH
Diskin, GS
Moore, RH
Thornhill, KL
Winstead, EL
Anderson, BE
AF Beyersdorf, A. J.
Ziemba, L. D.
Chen, G.
Corr, C. A.
Crawford, J. H.
Diskin, G. S.
Moore, R. H.
Thornhill, K. L.
Winstead, E. L.
Anderson, B. E.
TI The impacts of aerosol loading, composition, and water uptake on aerosol
extinction variability in the Baltimore-Washington, DC region
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID UNITED-STATES; DISCOVER-AQ; AIR-QUALITY; PM2.5; ABSORPTION; PROFILES;
HUMIDITY; AIRBORNE; MASS
AB In order to utilize satellite-based aerosol measurements for the determination of air quality, the relationship between aerosol optical properties (wavelength-dependent, column-integrated extinction measured by satellites) and mass measurements of aerosol loading (PM2.5 used for air quality monitoring) must be understood. This connection varies with many factors including those specific to the aerosol type - such as composition, size, and hygroscopicity - and to the surrounding atmosphere, such as temperature, relative humidity (RH), and altitude, all of which can vary spatially and temporally. During the DISCOVER-AQ (Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality) project, extensive in situ atmospheric profiling in the Baltimore, MD-Washington, D.C. region was performed during 14 flights in July 2011. Identical flight plans and profile locations throughout the project provide meaningful statistics for determining the variability in and correlations between aerosol loading, composition, optical properties, and meteorological conditions.
Measured water-soluble aerosol mass was composed primarily of ammonium sulfate (campaign average of 32 %) and organics (57 %). A distinct difference in composition was observed, with high-loading days having a proportionally larger percentage of sulfate due to transport from the Ohio River Valley. This composition shift caused a change in the aerosol water-uptake potential (hygroscopicity) such that higher relative contributions of inorganics increased the bulk aerosol hygroscopicity. These days also tended to have higher relative humidity, causing an increase in the water content of the aerosol. Conversely, low-aerosol-loading days had lower sulfate and higher black carbon contributions, causing lower single-scattering albedos (SSAs). The average black carbon concentrations were 240 ngm(-3) in the lowest 1 km, decreasing to 35 ngm(-3) in the free troposphere (above 3 km).
Routine airborne sampling over six locations was used to evaluate the relative contributions of aerosol loading, composition, and relative humidity (the amount of water available for uptake onto aerosols) to variability in mixed-layer aerosol extinction. Aerosol loading (dry extinction) was found to be the predominant source, accounting for 88 % on average of the measured spatial variability in ambient extinction, with lesser contributions from variability in relative humidity (10 %) and aerosol composition (1.3 %). On average, changes in aerosol loading also caused 82 % of the diurnal variability in ambient aerosol extinction. However on days with relative humidity above 60 %, variability in RH was found to cause up to 62 % of the spatial variability and 95 % of the diurnal variability in ambient extinction.
This work shows that extinction is driven to first order by aerosol mass loadings; however, humidity-driven hydration effects play an important secondary role. This motivates combined satellite-modeling assimilation products that are able to capture these components of the aerosol optical depth (AOD)-PM2.5 link. Conversely, aerosol hygroscopicity and SSA play a minor role in driving variations both spatially and throughout the day in aerosol extinction and therefore AOD. However, changes in aerosol hygroscopicity from day to day were large and could cause a bias of up to 27% if not accounted for. Thus it appears that a single daily measurement of aerosol hygroscopicity can be used for AOD-to-PM2.5 conversions over the study region (on the order of 1400 km(2)). This is complimentary to the results of Chu et al. (2015), who determined that the aerosol vertical distribution from "a single lidar is feasible to cover the range of 100 km" in the same region.
C1 [Beyersdorf, A. J.; Ziemba, L. D.; Chen, G.; Corr, C. A.; Crawford, J. H.; Diskin, G. S.; Moore, R. H.; Thornhill, K. L.; Winstead, E. L.; Anderson, B. E.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Corr, C. A.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Thornhill, K. L.; Winstead, E. L.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Beyersdorf, AJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM andreas.j.beyersdorf@nasa.gov
FU NASA's Earth Venture-1 Program through Earth System Science Pathfinder
(ESSP) Program Office
FX This research was funded by NASA's Earth Venture-1 Program through the
Earth System Science Pathfinder (ESSP) Program Office. We thank the
DISCOVER-AQ Science Team, especially the pilots and flight crews of
NASA's P-3B. Boundary layer heights based on airborne measurements of
the potential temperature profile were provided by Don Lenschow of the
University Corporation for Atmospheric Research (UCAR). Thanks also to
Joshua DiGangi and Michael Shook (both of NASA Langley) for valuable
discussions during manuscript preparation.
NR 32
TC 0
Z9 0
U1 18
U2 18
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 2
BP 1003
EP 1015
DI 10.5194/acp-16-1003-2016
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YH
UT WOS:000371284000032
ER
PT J
AU Xiao, Q
Zhang, H
Choi, M
Li, S
Kondragunta, S
Kim, J
Holben, B
Levy, RC
Liu, Y
AF Xiao, Q.
Zhang, H.
Choi, M.
Li, S.
Kondragunta, S.
Kim, J.
Holben, B.
Levy, R. C.
Liu, Y.
TI Evaluation of VIIRS, GOCI, and MODIS Collection 6AOD retrievals against
ground sunphotometer observations over East Asia
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AEROSOL OPTICAL-THICKNESS; LEVEL PM2.5; LAND; CALIBRATION; INSTRUMENT;
POLLUTION; PRODUCTS; MONITOR; AERONET; DEPTH
AB Persistent high aerosol loadings together with extremely high population densities have raised serious air quality and public health concerns in many urban centers in East Asia. However, ground-based air quality monitoring is relatively limited in this area. Recently, satellite-retrieved Aerosol Optical Depth (AOD) at high resolution has become a powerful tool to characterize aerosol patterns in space and time. Using ground AOD observations from the Aerosol Robotic Network (AERONET) and the Distributed Regional Aerosol Gridded Observation Networks (DRAGON)-Asia Campaign, as well as from handheld sunphotometers, we evaluated emerging aerosol products from the Visible Infrared Imaging Radiometer Suite (VIIRS) aboard the Suomi National Polar-orbiting Partnership (S-NPP), the Geostationary Ocean Color Imager (GOCI) aboard the Communication, Ocean, and Meteorology Satellite (COMS), and Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) (Collection 6) in East Asia in 2012 and 2013. In the case study in Beijing, when compared with AOD observations from handheld sunphotometers, 51% of VIIRS Environmental Data Record (EDR) AOD, 37% of GOCI AOD, 33% of VIIRS Intermediate Product (IP) AOD, 26% of Terra MODIS C6 3 km AOD, and 16% of Aqua MODIS C6 3 km AOD fell within the reference expected error (EE) envelope (+/- 0.05 +/- 0.15 AOD). Comparing against AERONET AOD over the Japan-South Korea region, 64% of EDR, 37% of IP, 61% of GOCI, 39% of Terra MODIS, and 56% of Aqua MODIS C6 3 km AOD fell within the EE. In general, satellite aerosol products performed better in tracking the day-to-day variability than tracking the spatial variability at high resolutions. The VIIRS EDR and GOCI products provided the most accurate AOD retrievals, while VIIRS IP and MODIS C6 3 km products had positive biases.
C1 [Xiao, Q.; Li, S.; Liu, Y.] Emory Univ, Rollins Sch Publ Hlth, Dept Environm Hlth, Atlanta, GA 30322 USA.
[Zhang, H.] IM Syst Grp Inc, College Pk, MD USA.
[Choi, M.; Kim, J.] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Li, S.] State Key Lab Remote Sensing Sci, Beijing, Peoples R China.
[Kondragunta, S.] NOAA, Greenbelt, MD USA.
[Holben, B.; Levy, R. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Liu, Y (reprint author), Emory Univ, Rollins Sch Publ Hlth, Dept Environm Hlth, Atlanta, GA 30322 USA.
EM yang.liu@emory.edu
RI Kondragunta, Shobha/F-5601-2010; Zhang, Hai/A-3445-2011; Levy,
Robert/M-7764-2013
OI Kondragunta, Shobha/0000-0001-8593-8046; Levy,
Robert/0000-0002-8933-5303
FU NASA Applied Sciences Program [NNX11AI53G, NNX14AG01G]; NASA EOS project
office; Ministry of Oceans and Fisheries, Korea; NASA Earth Science
Program [NNH13ZDA001N-TERAQEA]
FX The work of Y. Liu and Q. Xiao was partially supported by the NASA
Applied Sciences Program (grants NNX11AI53G and NNX14AG01G, PI: Liu). We
would like to acknowledge the AERONET team, I. Sano and the DRAGON-Japan
team, the Yonsi team and their collaborators in S. Korea, and CARSNET
and CAS teams in and around Beijing for providing data support in this
study. The AERONET project was supported by the NASA EOS project office,
and by Hal B. Maring, Radiation Sciences Program, NASA Headquarters.
This research was a part of the project titled "Research for
Applications of Geostationary Ocean Color Imager", funded by the
Ministry of Oceans and Fisheries, Korea. The MODIS project was supported
by the NASA Earth Science Program, grant NNH13ZDA001N-TERAQEA.
NR 28
TC 3
Z9 3
U1 8
U2 19
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 3
BP 1255
EP 1269
DI 10.5194/acp-16-1255-2016
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YI
UT WOS:000371284100004
ER
PT J
AU Schuster, GL
Dubovik, O
Arola, A
AF Schuster, G. L.
Dubovik, O.
Arola, A.
TI Remote sensing of soot carbon - Part 1: Distinguishing different
absorbing aerosol species
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID SKY BRIGHTNESS MEASUREMENTS; BIOMASS BURNING PARTICLES; COMPLEX
REFRACTIVE-INDEX; OPTICAL-PROPERTIES; LIGHT-ABSORPTION; BLACK CARBON;
ORGANIC-CARBON; BROWN CARBON; MINERALOGICAL COMPOSITION; RADIANCE
MEASUREMENTS
AB We describe a method of using the Aerosol Robotic Network (AERONET) size distributions and complex refractive indices to retrieve the relative proportion of carbonaceous aerosols and free iron minerals (hematite and goethite). We assume that soot carbon has a spectrally flat refractive index and enhanced imaginary indices at the 440 nm wavelength are caused by brown carbon or hematite. Carbonaceous aerosols can be separated from dust in imaginary refractive index space because 95% of biomass burning aerosols have imaginary indices greater than 0.0042 at the 675-1020 nm wavelengths, and 95% of dust has imaginary refractive indices of less than 0.0042 at those wavelengths. However, mixtures of these two types of particles can not be unambiguously partitioned on the basis of optical properties alone, so we also separate these particles by size. Regional and seasonal results are consistent with expectations. Monthly climatologies of fine mode soot carbon are less than 1.0% by volume for West Africa and the Middle East, but the southern African and South American biomass burning sites have peak values of 3.0 and 1.7 %. Monthly averaged fine mode brown carbon volume fractions have a peak value of 5.8% for West Africa, 2.1% for the Middle East, 3.7% for southern Africa, and 5.7% for South America. Monthly climatologies of free iron volume fractions show little seasonal variability, and range from about 1.1 to 1.7% for coarse mode aerosols in all four study regions. Finally, our sensitivity study indicates that the soot carbon retrieval is not sensitive to the component refractive indices or densities assumed for carbonaceous and free iron aerosols, and the retrieval differs by only 15.4% when these parameters are altered from our chosen baseline values. The total uncertainty of retrieving soot carbon mass is similar to 50% (when uncertainty in the AERONET product and mixing state is included in the analysis).
C1 [Schuster, G. L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Dubovik, O.] Univ Lille 1, Opt Atmospher Lab, CNRS, F-59655 Villeneuve Dascq, France.
[Arola, A.] Finnish Meteorol Inst, Kuopio, Finland.
RP Schuster, GL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM gregory.l.schuster@nasa.gov
OI Arola, Antti/0000-0002-9220-0194
FU National Aeronautics and Space Administration under NASA Glory Science
Team; Academy of Finland [264242]; Labex CaPPA project involving several
research institutions in Nord-Pasde-Calais, France
FX This material was supported by the National Aeronautics and Space
Administration under the NASA Glory Science Team, issued through the
Science Mission Directorate, Earth Science Division. Oleg Dubovik was
supported by the Labex CaPPA project involving several research
institutions in Nord-Pasde-Calais, France. Antti Arola acknowledges
support from the Academy of Finland (through the project number 264242).
We enjoyed informative discussions with Brent Holben and Tom Eck about
the AERONET products, and we appreciate the efforts of the 29 AERONET
and PHOTONS (Service d'Observation from LOA/USTL/CNRS) principal
investigators and the entire AERONET and PHOTONS teams for obtaining,
processing, documenting, and disseminating their respective data sets.
We also appreciate the thorough efforts of the four expert reviewers, as
their input greatly improved the final version of this paper. Finally,
we acknowledge the efforts of Phillip Stier for overseeing the review
process.
NR 86
TC 7
Z9 7
U1 10
U2 19
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 3
BP 1565
EP 1585
DI 10.5194/acp-16-1565-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YI
UT WOS:000371284100023
ER
PT J
AU Schuster, GL
Dubovik, O
Arola, A
Eck, TF
Holben, BN
AF Schuster, G. L.
Dubovik, O.
Arola, A.
Eck, T. F.
Holben, B. N.
TI Remote sensing of soot carbon - Part 2: Understanding the absorption
Angstrom exponent
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AEROSOL OPTICAL-PROPERTIES; SKY RADIANCE MEASUREMENTS; IN-SITU
MEASUREMENTS; LIGHT-ABSORPTION; BROWN CARBON; BLACK CARBON;
ORGANIC-CARBON; WAVELENGTH DEPENDENCE; SPECTRAL DEPENDENCE; MINERAL DUST
AB Recently, some authors have suggested that the absorption Angstrom exponent (AAE) can be used to deduce the component aerosol absorption optical depths (AAODs) of carbonaceous aerosols in the AERONET database. This AAE approach presumes that AAE << 1 for soot carbon, which contrasts the traditional small particle limit of AAE = 1 for soot carbon. Thus, we provide an overview of the AERONET retrieval, and we investigate how the microphysics of carbonaceous aerosols can be interpreted in the AERONET AAE product. We find that AAE << 1 in the AERONET database requires large coarse mode fractions and/or imaginary refractive indices that increase with wavelength. Neither of these characteristics are consistent with the current definition of soot carbon, so we explore other possibilities for the cause of AAE << 1. AAE is related to particle size, and coarse mode particles have a smaller AAE than fine mode particles for a given aerosol mixture of species. We also note that the mineral goethite has an imaginary refractive index that increases with wavelength, is very common in dust regions, and can easily contribute to AAE << 1. We find that AAE << 1 can not be caused by soot carbon, unless soot carbon has an imaginary refractive index that increases with wavelength throughout the visible and near-infrared spectrums. Finally, AAE is not a robust parameter for separating carbonaceous absorption from dust aerosol absorption in the AERONET database.
C1 [Schuster, G. L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Dubovik, O.] Univ Lille 1, Opt Atmospher Lab, CNRS, F-59655 Villeneuve Dascq, France.
[Arola, A.] Finnish Meteorol Inst, POB 1627, Kuopio 70211, Finland.
[Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA.
[Eck, T. F.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Schuster, GL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM gregory.l.schuster@nasa.gov
OI Arola, Antti/0000-0002-9220-0194
FU National Aeronautics and Space Administration under the NASA Glory
Science Team; Academy of Finland [264242]
FX This material was supported by the National Aeronautics and Space
Administration under the NASA Glory Science Team, issued through the
Science Mission Directorate, Earth Science Division. Oleg Dubovik was
supported by the Labex CaPPA project involving several research
institutions in Nord-Pasde-Calais, France. Antti Arola acknowledges
support from the Academy of Finland (through the project number 264242).
We appreciate the efforts of the 29 AERONET and PHOTONS (Service
d'Observation from LOA/USTL/CNRS) principal investigators and the entire
AERONET and PHOTONS teams for obtaining, processing, documenting, and
disseminating their respective data sets. Finally, we thank the
anonymous reviewers for their time and effort.
NR 101
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Z9 4
U1 6
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 3
BP 1587
EP 1602
DI 10.5194/acp-16-1587-2016
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YI
UT WOS:000371284100024
ER
PT J
AU Marais, EA
Jacob, DJ
Jimenez, JL
Campuzano-Jost, P
Day, DA
Hu, W
Krechmer, J
Zhu, L
Kim, PS
Miller, CC
Fisher, JA
Travis, K
Yu, K
Hanisco, TF
Wolfe, GM
Arkinson, HL
Pye, HOT
Froyd, KD
Liao, J
McNeill, VF
AF Marais, E. A.
Jacob, D. J.
Jimenez, J. L.
Campuzano-Jost, P.
Day, D. A.
Hu, W.
Krechmer, J.
Zhu, L.
Kim, P. S.
Miller, C. C.
Fisher, J. A.
Travis, K.
Yu, K.
Hanisco, T. F.
Wolfe, G. M.
Arkinson, H. L.
Pye, H. O. T.
Froyd, K. D.
Liao, J.
McNeill, V. F.
TI Aqueous-phase mechanism for secondary organic aerosol formation from
isoprene: application to the southeast United States and co-benefit of
SO2 emission controls
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID HIGH-NOX CONDITIONS; REACTIVE UPTAKE; RELATIVE-HUMIDITY; ANTHROPOGENIC
EMISSIONS; 2-METHYLGLYCERIC ACID; ATMOSPHERIC AEROSOLS;
MASS-SPECTROMETER; EPOXIDE FORMATION; RATE CONSTANTS; NORTH-AMERICA
AB Isoprene emitted by vegetation is an important precursor of secondary organic aerosol (SOA), but the mechanism and yields are uncertain. Aerosol is prevailingly aqueous under the humid conditions typical of isoprene-emitting regions. Here we develop an aqueous-phase mechanism for isoprene SOA formation coupled to a detailed gas-phase isoprene oxidation scheme. The mechanism is based on aerosol reactive uptake coefficients (gamma) for water-soluble isoprene oxidation products, including sensitivity to aerosol acidity and nucleophile concentrations. We apply this mechanism to simulation of aircraft (SEAC(4)RS) and ground-based (SOAS) observations over the southeast US in summer 2013 using the GEOS-Chem chemical transport model. Emissions of nitrogen oxides (NOx = NO + NO2) over the southeast US are such that the peroxy radicals produced from isoprene oxidation (ISOPO2) react significantly with both NO (high-NOx pathway) and HO2 (low-NOx pathway), leading to different suites of isoprene SOA precursors. We find a mean SOA mass yield of 3.3% from isoprene oxidation, consistent with the observed relationship of total fine organic aerosol (OA) and formaldehyde (a product of isoprene oxidation). Isoprene SOA production is mainly contributed by two immediate gasphase precursors, isoprene epoxydiols (IEPOX, 58% of isoprene SOA) from the low-NOx pathway and glyoxal (28 %) from both low-and high-NOx pathways. This speciation is consistent with observations of IEPOX SOA from SOAS and SEAC4RS. Observations show a strong relationship between IEPOX SOA and sulfate aerosol that we explain as due to the effect of sulfate on aerosol acidity and volume. Isoprene SOA concentrations increase as NOx emissions decrease (favoring the low-NOx pathway for isoprene oxidation), but decrease more strongly as SO2 emissions decrease (due to the effect of sulfate on aerosol acidity and volume). The US Environmental Protection Agency (EPA) projects 2013-2025 decreases in anthropogenic emissions of 34% for NOx (leading to a 7% increase in isoprene SOA) and 48% for SO2 (35% decrease in isoprene SOA). Reducing SO2 emissions decreases sulfate and isoprene SOA by a similar magnitude, representing a factor of 2 co-benefit for PM2.5 from SO2 emission controls.
C1 [Marais, E. A.; Jacob, D. J.; Zhu, L.; Travis, K.; Yu, K.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Jacob, D. J.; Kim, P. S.; Miller, C. C.] Harvard Univ, Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Jimenez, J. L.; Campuzano-Jost, P.; Day, D. A.; Hu, W.; Krechmer, J.; Froyd, K. D.; Liao, J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Jimenez, J. L.; Campuzano-Jost, P.; Day, D. A.; Hu, W.; Krechmer, J.] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Fisher, J. A.] Univ Wollongong, Sch Chem, Wollongong, NSW, Australia.
[Fisher, J. A.] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW, Australia.
[Hanisco, T. F.; Wolfe, G. M.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Wolfe, G. M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Arkinson, H. L.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Pye, H. O. T.] US EPA, Natl Exposure Res Lab, Res Triangle Pk, NC 27711 USA.
[Froyd, K. D.; Liao, J.] NOAA, Earth Syst Res Lab, Chem Sci Div, Boulder, CO USA.
[McNeill, V. F.] Columbia Univ, Dept Chem Engn, New York, NY USA.
RP Marais, EA (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
EM emarais@seas.harvard.edu
RI Jimenez, Jose/A-5294-2008; Wolfe, Glenn/D-5289-2011; Travis,
Katherine/G-1417-2016; Fisher, Jenny/J-3979-2012; Pye,
Havala/F-5392-2012; Krechmer, Jordan/C-9153-2016; Chem,
GEOS/C-5595-2014; Manager, CSD Publications/B-2789-2015;
OI Jimenez, Jose/0000-0001-6203-1847; Travis,
Katherine/0000-0003-1628-0353; Fisher, Jenny/0000-0002-2921-1691; Pye,
Havala/0000-0002-2014-2140; Krechmer, Jordan/0000-0003-3642-0659;
Marais, Eloise/0000-0001-5477-8051
FU NASA Tropospheric Chemistry Program; NASA Air Quality Applied Sciences
Team; South African National Research Foundation Fellowship;
Schlumberger Faculty for the Future Fellowship
FX We are grateful to the entire NASA SEAC4RS team for their
help in the field, in particular Paul Wennberg, John Crounse, Jason St.
Clair, and Alex Teng for their CIT-CIMS measurements. Thanks also to
Jesse Kroll for assisting in the interpretation of chamber study
results. This work was funded by the NASA Tropospheric Chemistry
Program, the NASA Air Quality Applied Sciences Team, and a South African
National Research Foundation Fellowship and Schlumberger Faculty for the
Future Fellowship to E. A. Marais. W. Hu, J. Krechmer, P.
Campuzano-Jost, D. A. Day, and J. L. Jimenez were supported by NASA
NNX12AC03G/NNX15AT96G and NSF AGS-1243354. J. Krechmer was supported by
EPA STAR (FP-91770901-0) and CIRES Fellowships. J. A. Fisher
acknowledges support from a University of Wollongong Vice Chancellor's
Postdoctoral Fellowship. HCHO observations were acquired with support
from NASA ROSES SEAC4RS grant NNH10ZDA001N. Although this
document has been reviewed by US EPA and approved for publication, it
does not necessarily reflect US EPA's policies or views.
NR 113
TC 15
Z9 15
U1 31
U2 61
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 3
BP 1603
EP 1618
DI 10.5194/acp-16-1603-2016
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YI
UT WOS:000371284100025
ER
PT J
AU Kim, M
Kim, J
Jeong, U
Kim, W
Hong, H
Holben, B
Eck, TF
Lim, JH
Song, CK
Lee, S
Chung, CY
AF Kim, M.
Kim, J.
Jeong, U.
Kim, W.
Hong, H.
Holben, B.
Eck, T. F.
Lim, J. H.
Song, C. K.
Lee, S.
Chung, C. -Y.
TI Aerosol optical properties derived from the DRAGON-NE Asia campaign, and
implications for a single-channel algorithm to retrieve aerosol optical
depth in spring from Meteorological Imager (MI) on-board the
Communication, Ocean, and Meteorological Satellite (COMS)
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; RADIATIVE-TRANSFER CODE; GEOSTATIONARY
SATELLITE; SURFACE REFLECTANCE; ATMOSPHERIC CORRECTION; VECTOR VERSION;
SOURCE REGIONS; HONG-KONG; ACE-ASIA; PART I
AB An aerosol model optimized for northeast Asia is updated with the inversion data from the Distributed Regional Aerosol Gridded Observation Networks (DRAGON)northeast (NE) Asia campaign which was conducted during spring from March to May 2012. This updated aerosol model was then applied to a single visible channel algorithm to retrieve aerosol optical depth (AOD) from a Meteorological Imager (MI) on-board the geostationary meteorological satellite, Communication, Ocean, and Meteorological Satellite (COMS). This model plays an important role in retrieving accurate AOD from a single visible channel measurement. For the single-channel retrieval, sensitivity tests showed that perturbations by 4% (0.926 +/- 0.04) in the assumed single scattering albedo (SSA) can result in the retrieval error in AOD by over 20 %. Since the measured reflectance at the top of the atmosphere depends on both AOD and SSA, the overestimation of assumed SSA in the aerosol model leads to an underestimation of AOD. Based on the AErosol RObotic NETwork (AERONET) inversion data sets obtained over East Asia before 2011, seasonally analyzed aerosol optical properties (AOPs) were categorized by SSAs at 675 nm of 0.92 +/- 0.035 for spring (March, April, and May). After the DRAGON-NE Asia campaign in 2012, the SSA during spring showed a slight increase to 0.93 +/- 0.035. In terms of the volume size distribution, the mode radius of coarse particles was increased from 2.08 +/- 0.40 to 2.14 +/- 0.40. While the original aerosol model consists of volume size distribution and refractive indices obtained before 2011, the new model is constructed by using a total data set after the DRAGON-NE Asia campaign. The large volume of data in high spatial resolution from this intensive campaign can be used to improve the representative aerosol model for East Asia. Accordingly, the new AOD data sets retrieved from a single-channel algorithm, which uses a precalculated look-up table (LUT) with the new aerosol model, show an improved correlation with the measured AOD during the DRAGON-NE Asia campaign. The correlation between the new AOD and AERONET value shows a regression slope of 1.00, while the comparison of the original AOD data retrieved using the original aerosol model shows a slope of 1.08. The change of y-offset is not significant, and the correlation coefficients for the comparisons of the original and new AOD are 0.87 and 0.85, respectively. The tendency of the original aerosol model to overestimate the retrieved AOD is significantly improved by using the SSA values in addition to size distribution and refractive index obtained using the new model.
C1 [Kim, M.; Kim, J.; Jeong, U.; Kim, W.] Yonsei Univ, Dept Atmospher Sci IEAA BK Plus 21, Seoul 120749, South Korea.
[Hong, H.] Pukyong Natl Univ, Dept Spatial Informat Engn, Busan, South Korea.
[Holben, B.; Eck, T. F.] NASA Goddard Space Flight, Greenbelt, MD USA.
[Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA.
[Lim, J. H.; Song, C. K.; Lee, S.] NIER, Inchon, South Korea.
[Chung, C. -Y.] Nat Meteorol Satellite Ctr, Gwanghyewon myeon, Jincheon Gun, Chungcheongbuk, South Korea.
[Lee, S.] Asia Ctr Air Pollut Res ACAP, Niigata, Japan.
RP Kim, J (reprint author), Yonsei Univ, Dept Atmospher Sci IEAA BK Plus 21, Seoul 120749, South Korea.
EM jkim2@yonsei.ac.kr
RI Song, Chang-Keun/S-2255-2016
OI Song, Chang-Keun/0000-0002-8811-2626
FU GEMS program of Ministry of Environment, Korea; Eco Innovation Program
of KEITI [2012000160002]; Brain Korea 21 Plus
FX We thank the principal investigators and their staff for establishing
and maintaining the AERONET sites used in this investigation. We also
gratefully acknowledge the principal investigator and staff of the
DRAGON-NE Asia campaign for their effort. This research was supported by
the GEMS program of the Ministry of Environment, Korea, and the Eco
Innovation Program of KEITI (2012000160002). This research was partially
supported by the Brain Korea 21 Plus (J. Kim and M. Kim).
NR 54
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Z9 0
U1 1
U2 3
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PY 2016
VL 16
IS 3
BP 1789
EP 1808
DI 10.5194/acp-16-1789-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DF3YI
UT WOS:000371284100036
ER
PT J
AU Kwok, R
Morison, J
AF Kwok, Ron
Morison, James
TI Sea surface height and dynamic topography of the ice-covered oceans from
CryoSat-2: 2011-2014
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE sea surface height; dynamic topography; Arctic Ocean; Southern Ocean
ID ARCTIC-OCEAN; GRACE; GRAVITY; ALTIMETRY; PATHWAYS; LAND
AB We examine 4 years (2011-2014) of sea surface heights (SSH) from CryoSat-2 (CS-2) over the ice-covered Arctic and Southern Oceans. Results are from a procedure that identifies and determines the heights of sea surface returns. Along 25 km segments of satellite ground tracks, variability in the retrieved SSHs is between similar to 2 and 3 cm (standard deviation) in the Arctic and is slightly higher (similar to 3 cm) in the summer and the Southern Ocean. Average sea surface tilts (along these 25 km segments) are 0.013.8 cm/10 km in the Arctic, and slightly lower (0.012.0 cm/10 km) in the Southern Ocean. Intra-seasonal variability of CS-2 dynamic ocean topography (DOT) in the ice-covered Arctic is nearly twice as high as that of the Southern Ocean. In the Arctic, we find a correlation of 0.92 between 3 years of DOT and dynamic heights (DH) from hydrographic stations. Further, correlation of 4 years of area-averaged CS-2 DOT near the North Pole with time-variable ocean-bottom pressure from a pressure gauge and from GRACE, yields coefficients of 0.83 and 0.77, with corresponding differences of <3 cm (RMS). These comparisons contrast the length scale of baroclinic and barotropic features and reveal the smaller amplitude barotropic signals in the Arctic Ocean. Broadly, the mean DOT from CS-2 for both poles compares well with those from the ICESat campaigns and the DOT2008A and DTU13MDT fields. Short length scale topographic variations, due to oceanographic signals and geoid residuals, are especially prominent in the Arctic Basin but less so in the Southern Ocean.
C1 [Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Morison, James] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NASA [NNX13AP72G, NNX12AK74G]; NSF [ARC-0856330]
FX GRACE ocean data were processed by Don P. Chambers, supported by the
NASA MEaSUREs Program, and are available at http://grace.jpl.nasa.gov.
Suzanne Dickinson has calculated the correlations of the CS-2 DOT with
Arctic dynamic heights and Cecilia Peralta-Ferriz has provided the North
Pole ABPR data. The work at the Polar Science Center was supported by
NASA grants NNX13AP72G and NNX12AK74G and NSF grant ARC-0856330. RK
carried out this work at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 44
TC 1
Z9 1
U1 5
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD JAN
PY 2016
VL 121
IS 1
BP 674
EP 692
DI 10.1002/2015JC011357
PG 19
WC Oceanography
SC Oceanography
GA DF5ZH
UT WOS:000371432200039
ER
PT J
AU Overholt, EP
Rose, KC
Williamson, CE
Fischer, JM
Cabrol, NA
AF Overholt, Erin P.
Rose, Kevin C.
Williamson, Craig E.
Fischer, Janet M.
Cabrol, Nathalie A.
TI Behavioral responses of freshwater calanoid copepods to the presence of
ultraviolet radiation: avoidance and attraction
SO JOURNAL OF PLANKTON RESEARCH
LA English
DT Article
DE zooplankton; UV; behavior; lake; transparency
ID DIEL VERTICAL MIGRATION; CARIBBEAN SPINY LOBSTERS; SOLAR UV-RADIATION;
HIGH-MOUNTAIN LAKE; TRANSPARENCY-GRADIENT; SPECTRAL SENSITIVITY;
DAPHNIA-MAGNA; ZOOPLANKTON; PREDATION; LIGHT
AB Binary choice experiments under natural solar radiation were used to test short-term behavioral responses of freshwater calanoid copepods to ultraviolet radiation (UV). Responses of the nine species from 15 populations spanning North and South America included both UV attraction and UV avoidance, and varied among habitats, species and populations. Copepods from more transparent lakes were more attracted to UV than those from less transparent lakes. When individuals were pre-exposed in the laboratory to photosynthetically active radiation (PAR) in the presence and absence of UV, those pre-exposed to UV spent more time in the high UV environment than those exposed to PAR alone. However, these differences disappeared after 150 min, suggesting that the responses were short term and mediated in part by ambient UV conditions. Copepods represent a large proportion of the biomass of zooplankton in many aquatic ecosystems, and their ability to detect and respond behaviorally to UV may enable them to use this ubiquitous environmental cue to regulate their water column position. The use of UV as a habitat selection cue may permit copepods to exploit optimal food environments or limit overlap with less UV-tolerant competitors, predators or parasites, while minimizing damage resulting from longer term UV exposure.
C1 [Overholt, Erin P.; Rose, Kevin C.; Williamson, Craig E.] Miami Univ, Dept Biol, Oxford, OH 45056 USA.
[Fischer, Janet M.] Franklin & Marshall Coll, Dept Biol, Lancaster, PA 17604 USA.
[Cabrol, Nathalie A.] NASA Ames, Seti Inst Carl Sagan Ctr, Ames, CA USA.
[Rose, Kevin C.] Rensselaer Polytech Inst, Dept Biol Sci, Troy, NY USA.
RP Overholt, EP (reprint author), Miami Univ, Dept Biol, Oxford, OH 45056 USA.
EM overhoep@miamioh.edu
FU National Science Foundation (NSF) Division of Environmental Biology
(DEB) [0734277]; Miami University; Smithsonian Institution; Franklin and
Marshall College; Andrew W. Mellon Foundation; NASA Astrobiology
Institute (High Lakes Project); NASA Astrobiology Science and Technology
for Exploring Planets (NASA ASTEP)
FX This work was supported by the National Science Foundation (NSF)
Division of Environmental Biology (DEB) (grant number 0734277 to [K.C.R.
and C.E.W.]); Miami University to [K.C.R., C.E.W. and E.P.O.];
Smithsonian Institution to [K.C.R.]; Franklin and Marshall College to
[J.M.F.]; Andrew W. Mellon Foundation to [J.M.F.]; NASA Astrobiology
Institute (High Lakes Project to [N.C.]); and NASA Astrobiology Science
and Technology for Exploring Planets (NASA ASTEP) (Planetary Lake Lander
to [N.C.]).
NR 60
TC 4
Z9 4
U1 6
U2 17
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0142-7873
EI 1464-3774
J9 J PLANKTON RES
JI J. Plankton Res.
PD JAN-FEB
PY 2016
VL 38
IS 1
BP 16
EP 26
DI 10.1093/plankt/fbv113
PG 11
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA DF3FR
UT WOS:000371229900003
ER
PT J
AU Mouroulis, P
Green, RO
Van Gorp, B
Moore, LB
Wilson, DW
Bender, HA
AF Mouroulis, Pantazis
Green, Robert O.
Van Gorp, Byron
Moore, Lori B.
Wilson, Daniel W.
Bender, Holly A.
TI Landsat swath imaging spectrometer design
SO OPTICAL ENGINEERING
LA English
DT Article
DE imaging spectrometer; Landsat; visible to short-wave infrared; Dyson
spectrometer
AB This paper describes the design of a high-throughput and high-uniformity pushbroom imaging spectrometer and telescope system that is capable of Landsat swath and resolution while providing better than 10 nm per pixel spectral resolution over the full visible to short-wave infrared band. The design is based on a 3200 x 480 element x 18 mu mpixel size focal plane array, two of which are utilized to cover the full swath. At an optical speed of F/1.8, the system is the fastest proposed to date to our knowledge. The utilization of only two Dyson-type spectrometer modules fed from the same telescope reduces system complexity while providing a solution within achievable detector technology. Two telescope designs are shown to achieve the required swath and resolution from different altitudes. Predictions of complete system response are shown. Also, it is shown that detailed ghost analysis is a requirement for this type of spectrometer and forms an essential part of a complete design. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Mouroulis, Pantazis; Green, Robert O.; Van Gorp, Byron; Moore, Lori B.; Wilson, Daniel W.; Bender, Holly A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pantazis.mouroulis@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was performed at the Jet Propulsion Laboratory, California
Institute of Technology under a contract with the National Aeronautics
and Space Administration. Reference herein to any specific commercial
product, process, or service by trade name, trademark, manufacturer, or
otherwise, does not constitute or imply its endorsement by the United
States Government or the Jet Propulsion Laboratory, California Institute
of Technology.
NR 25
TC 1
Z9 1
U1 1
U2 6
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD JAN
PY 2016
VL 55
IS 1
AR 015104
DI 10.1117/1.OE.55.1.015104
PG 11
WC Optics
SC Optics
GA DF3YC
UT WOS:000371283500027
ER
PT J
AU Kumar-Krishnan, S
Chakaravarthy, S
Hernandez-Rangel, A
Prokhorov, E
Luna-Barcenas, G
Esparza, R
Meyyappan, M
AF Kumar-Krishnan, Siva
Chakaravarthy, S.
Hernandez-Rangel, A.
Prokhorov, E.
Luna-Barcenas, G.
Esparza, Rodrigo
Meyyappan, M.
TI Chitosan supported silver nanowires as a platform for direct
electrochemistry and highly sensitive electrochemical glucose biosensing
SO RSC ADVANCES
LA English
DT Article
ID DIRECT ELECTRON-TRANSFER; MICROBIAL FUEL-CELLS; CARBON NANOTUBE;
COMPOSITE FILM; REDOX ENZYMES; OXIDASE; IMMOBILIZATION; NANOPARTICLES;
PROTEINS; TIO2
AB The development of low-cost and sensitive glucose biosensors has been the focus of substantial research interest due to their diverse applications in medical diagnosis, healthcare, and environmental monitoring. Herein, we report the successful use of chitosan (CS) supported silver nanowires (AgNWs) based enzyme electrodes for highly sensitive electrochemical glucose biosensing. The glucose oxidase (GOx) enzyme is electrically contacted using highly conductive AgNWs and thereby significant enhancement in the direct electron transfer (DET) between the redox enzymes and the electrode surface. In addition, the CS polymer matrix enables distinct self-assembly of GOx enzymes adjacent to the electrode surface, which further favours DET by increasing the charge transfer. Characterization by Fourier transform infrared (FTIR) spectroscopy and atomic force microscopy (AFM) measurements were used to evidence the intermolecular interaction and self-assembly of the GOx on CS polymers. AFM results clearly revealed the self-assembly of the GOx on CS surfaces. The immobilized GOx exhibits a well-defined quasi-reversible redox peak with an electron rate constant (k(s)) of 6.52 s(-1) compared to the bare glassy carbon electrode (GCE). The resultant biosensor demonstrates a high sensitivity of 16.72 mu A mM(-1) cm(-2) with a wide linear range (1-15 mM), good selectivity and long-term stability for glucose detection. Our current approach represents a promising platform for the immobilization and electrical wiring of biomolecules with higher loading efficiency for designing low-cost, high sensitive enzymatic biosensors.
C1 [Kumar-Krishnan, Siva; Hernandez-Rangel, A.; Prokhorov, E.; Luna-Barcenas, G.] Cinvestav Queretaro, Queretaro 76230, Qro, Mexico.
[Kumar-Krishnan, Siva; Esparza, Rodrigo] Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Blvd Juriquilla 3001, Santiago De Queretaro 76230, Qro, Mexico.
[Chakaravarthy, S.] IPN, CINVESTAV, Programa Doctorado Nanociencias & Nanotecnol, Mexico City 07360, DF, Mexico.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kumar-Krishnan, S; Luna-Barcenas, G (reprint author), Cinvestav Queretaro, Queretaro 76230, Qro, Mexico.; Kumar-Krishnan, S (reprint author), Univ Nacl Autonoma Mexico, Ctr Fis Aplicada & Tecnol Avanzada, Blvd Juriquilla 3001, Santiago De Queretaro 76230, Qro, Mexico.
EM skumar@fata.unam.mx; glunascf@yahoo.com
FU DGAPA-UNAM post-doctoral fellowship
FX This work was supported by the DGAPA-UNAM post-doctoral fellowship. The
authors are grateful to J. A. Munoz-Salas for assistance in the
construction of GCE electrodes, Ma. Lourdes Palma Tirado (Campus UNAM
Juriquilla, Qro) for TEM measurements and C. I. Enriquez-Flores for the
help in AFM measurements.
NR 62
TC 4
Z9 4
U1 24
U2 58
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2046-2069
J9 RSC ADV
JI RSC Adv.
PY 2016
VL 6
IS 24
BP 20102
EP 20108
DI 10.1039/c5ra24259b
PG 7
WC Chemistry, Multidisciplinary
SC Chemistry
GA DF1TU
UT WOS:000371122900061
ER
PT J
AU Dai, Q
Han, DW
Zhuo, L
Zhang, J
Islam, T
Srivastava, PK
AF Dai, Qiang
Han, Dawei
Zhuo, Lu
Zhang, Jun
Islam, Tanvir
Srivastava, Prashant K.
TI Seasonal ensemble generator for radar rainfall using copula and
autoregressive model
SO STOCHASTIC ENVIRONMENTAL RESEARCH AND RISK ASSESSMENT
LA English
DT Article
DE Copula; Season; Synoptic regimes; Radar rainfall uncertainty
ID REAL-TIME CORRECTION; MEAN-FIELD BIAS; PRECIPITATION ESTIMATION;
MOUNTAINOUS REGION; BRIGHT-BAND; WIND-DRIFT; REFLECTIVITY; UNCERTAINTY;
SIMULATION; WSR-88D
AB Uncertainty analysis of radar rainfall enables stakeholders and users have a clear knowledge of the possible uncertainty associated with the rainfall products. Long-term empirical modeling of the relationship between radar and gauge measurements is an efficient and practical method to describe the radar rainfall uncertainty. However, complicated variation of synoptic conditions makes the radar-rainfall uncertainty model based on historical data hard to extend in the future state. A promising solution is to integrate synoptic regimes with the empirical model and explore the impact of individual synoptic regimes on radar rainfall uncertainty. This study is an attempt to introduce season, one of the most important synoptic factor, into the radar rainfall uncertainty model and proposes a seasonal ensemble generator for radar rainfall using copula and autoregressive model. We firstly analyze the histograms of rainfall-weighted temperature, the radar-gauge relationships, and Box and Whisker plots in different seasons and conclude that the radar rainfall uncertainty has strong seasonal dependence. Then a seasonal ensemble generator is designed and implemented in a UK catchment under a temperate maritime climate, which can fully model marginal distribution, spatial dependence, temporal dependence and seasonal dependence of radar rainfall uncertainty. To test its performance, 12 typical rainfall events (4 for each season) are chosen to generate ensemble rainfall values. In each time step, 500 ensemble members are produced and the values of 5th to 95th percentiles are used to derive the uncertainty bands. Except several outliers, the uncertainty bands encompass the observed gauge rainfall quite well. The parameters of the ensemble generator vary considerably for each season, indicating the seasonal ensemble generator reflects the impact of seasons on radar rainfall uncertainty. This study is an attempt to simultaneously consider four key features of radar rainfall uncertainty and future study will investigate their impacts on the outputs of hydrological models with radar rainfall as input or initial conditions.
C1 [Dai, Qiang] Nanjing Normal Univ, Sch Geog Sci, Minist Educ, Key Lab Virtual Geog Environm, Nanjing, Peoples R China.
[Dai, Qiang; Han, Dawei; Zhuo, Lu; Zhang, Jun] Univ Bristol, Dept Civil Engn, WEMRC, Bristol, Avon, England.
[Islam, Tanvir] NOAA NESDIS Ctr Satellite Applicat & Res, College Pk, MD USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Dai, Q (reprint author), Nanjing Normal Univ, Sch Geog Sci, Minist Educ, Key Lab Virtual Geog Environm, Nanjing, Peoples R China.
EM q.dai@bristol.ac.uk
OI Islam, Tanvir/0000-0003-2429-3074
FU University of Bristol; China Scholarship Council
FX The first author would like to thank the University of Bristol and China
Scholarship Council for providing the necessary support and funding for
his PhD research. The authors acknowledge the British Atmospheric Data
Centre for providing the data.
NR 49
TC 0
Z9 0
U1 5
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1436-3240
EI 1436-3259
J9 STOCH ENV RES RISK A
JI Stoch. Environ. Res. Risk Assess.
PD JAN
PY 2016
VL 30
IS 1
BP 27
EP 38
DI 10.1007/s00477-014-1017-x
PG 12
WC Engineering, Environmental; Engineering, Civil; Environmental Sciences;
Statistics & Probability; Water Resources
SC Engineering; Environmental Sciences & Ecology; Mathematics; Water
Resources
GA DF4KP
UT WOS:000371317300003
ER
PT J
AU Drikakis, D
Kwak, D
Kiris, CC
AF Drikakis, Dimitris
Kwak, Dochan
Kiris, Cetin C.
TI Computational aerodynamics: Advances and challenges
SO AERONAUTICAL JOURNAL
LA English
DT Article
DE CFD; aerodynamics; computational sciences
ID LARGE-EDDY SIMULATION; TURBULENT CHANNEL FLOW; DIRECT
NUMERICAL-SIMULATION; HYPERBOLIC CONSERVATION-LAWS; HYBRID RANS/LES
SIMULATION; HIGH-RESOLUTION SCHEMES; HIGH REYNOLDS-NUMBERS; LATTICE-GAS
AUTOMATA; WALL-BOUNDED FLOWS; IMPLICIT LES
AB Computational aerodynamics, which complement more expensive empirical approaches, are critical for developing aerospace vehicles. During the past three decades, computational aerodynamics capability has improved remarkably, following advances in computer hardware and algorithm development. However, most of the fundamental computational capability realised in recent applications is derived from earlier advances, where specific gaps in solution procedures have been addressed only incrementally. The present article presents our view of the state of the art in computational aerodynamics and assessment of the issues that drive future aerodynamics and aerospace vehicle development. Requisite capabilities for perceived future needs are discussed, and associated grand challenge problems are presented.
C1 [Drikakis, Dimitris] Univ Strathclyde, Glasgow, Lanark, Scotland.
[Kwak, Dochan; Kiris, Cetin C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Drikakis, D (reprint author), Univ Strathclyde, Glasgow, Lanark, Scotland.
NR 136
TC 0
Z9 0
U1 10
U2 17
PU ROYAL AERONAUTICAL SOC
PI LONDON
PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND
SN 0001-9240
J9 AERONAUT J
JI Aeronaut. J.
PD JAN
PY 2016
VL 120
IS 1223
SI SI
BP 13
EP 36
DI 10.1017/aer.2015.2
PG 24
WC Engineering, Aerospace
SC Engineering
GA DE7RN
UT WOS:000370834500003
ER
PT J
AU Alisic, L
Rhebergen, S
Rudge, JF
Katz, RF
Wells, GN
AF Alisic, Laura
Rhebergen, Sander
Rudge, John F.
Katz, Richard F.
Wells, Garth N.
TI Torsion of a cylinder of partially molten rock with a spherical
inclusion: Theory and simulation
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE mantle; partial melt; torsion; simulation; viscosity; two-phase flow
ID COUPLED MAGMA/MANTLE DYNAMICS; BLOCK PRECONDITIONERS; SHEAR
LOCALIZATION; VISCOUS ANISOTROPY; MELT SEGREGATION; PRESSURE SHADOWS;
CONSEQUENCES; DEFORMATION; COMPACTION; EQUATIONS
AB The processes that are involved in migration and extraction of melt from the mantle are not yet fully understood. Gaining a better understanding of material properties of partially molten rock could help shed light on the behavior of melt on larger scales in the mantle. In this study, we simulate three-dimensional torsional deformation of a partially molten rock that contains a rigid, spherical inclusion. We compare the computed porosity patterns to those found in recent laboratory experiments. The laboratory experiments show emergence of melt-rich bands throughout the rock sample, and pressure shadows around the inclusion. The numerical model displays similar melt-rich bands only for a small bulk-to-shear-viscosity ratio (five or less). The results are consistent with earlier two-dimensional numerical simulations; however, we show that it is easier to form melt-rich bands in three dimensions compared to two. The addition of strain-rate dependence of the viscosity causes a distinct change in the shape of pressure shadows around the inclusion. This change in shape presents an opportunity for experimentalists to identify the strain-rate dependence and therefore the dominant deformation mechanism in torsion experiments with inclusions.
C1 [Alisic, Laura; Rudge, John F.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.
[Alisic, Laura] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Rhebergen, Sander] Univ Waterloo, Dept Appl Math, Waterloo, ON N2L 3G1, Canada.
[Katz, Richard F.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England.
[Wells, Garth N.] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England.
RP Alisic, L (reprint author), Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.; Alisic, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Laura.A.Jewell@jpl.nasa.gov
OI Rhebergen, Sander/0000-0001-6036-0356; Katz, Richard/0000-0001-8746-5430
FU UK Natural Environment Research Council [NE/I023929/1, NE/I026995/1];
Leverhulme Trust
FX This work was supported by the UK Natural Environment Research Council
under grants NE/I023929/1 and NE/I026995/1. Computations were performed
on the ARCHER UK National Supercomputing Service
(http://www.archer.ac.uk). We thank Chris Richardson for all his support
with running the simulations on ARCHER. Katz thanks the Leverhulme Trust
for support.
NR 28
TC 1
Z9 1
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD JAN
PY 2016
VL 17
IS 1
BP 143
EP 161
DI 10.1002/2015GC006061
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DE4SN
UT WOS:000370620600010
ER
PT J
AU French, JE
Blake, DF
AF French, Jason E.
Blake, David F.
TI Discovery of Naturally Etched Fission Tracks and Alpha-Recoil Tracks in
Submarine Glasses: Reevaluation of a Putative Biosignature for Earth and
Mars
SO INTERNATIONAL JOURNAL OF GEOPHYSICS
LA English
DT Article
ID MARTIAN METEORITE ALH84001; ALTERED BASALTIC GLASS; BIOLOGICALLY
MEDIATED DISSOLUTION; MONTE-CARLO CALCULATION; MID-ATLANTIC RIDGE;
COSTA-RICA RIFT; VOLCANIC GLASS; OCEANIC-CRUST; ALTERATION TEXTURES;
RADIATION-DAMAGE
AB Over the last two decades, conspicuously "biogenic-looking" corrosion microtextures have been found to occur globally within volcanic glass of the in situ oceanic crust, ophiolites, and greenstone belts dating back to similar to 3.5Ga. These so-called "tubular" and "granular" microtextures are widely interpreted to represent bona fide microbial trace fossils; however, possible nonbiological origins for these complex alteration microtextures have yet to be explored. Here, we reevaluate the origin of these enigmatic microtextures from a strictly nonbiological standpoint, using a case study on submarine glasses from the western North Atlantic Ocean (DSDP 418A). By combining petrographic and SEM observations of corrosion microtextures at the glass-palagonite interface, considerations of the tectonic setting, measurement of U and Th concentrations of fresh basaltic glass by ICP-MS, and theoretical modelling of the present-day distribution of radiation damage in basaltic glass caused by radioactive decay of U and Th, we reinterpret these enigmatic microtextures as the end product of the preferential corrosion/dissolution of radiation damage (alpha-recoil tracks and fission tracks) in the glass by seawater, possibly combined with pressure solution etch-tunnelling. Our findings have important implications for geomicrobiology, astrobiological exploration of Mars, and understanding of the long-term breakdown of nuclear waste glass.
C1 [French, Jason E.] Univ Alberta, Dept Earth & Atmospher Sci, 1-26 Earth Sci Bldg, Edmonton, AB T6G 2E3, Canada.
[Blake, David F.] NASA, Ames Res Ctr, Exobiol Branch, MS 239-4, Moffett Field, CA 94035 USA.
RP French, JE (reprint author), Univ Alberta, Dept Earth & Atmospher Sci, 1-26 Earth Sci Bldg, Edmonton, AB T6G 2E3, Canada.
EM jef@ualberta.ca
NR 244
TC 0
Z9 0
U1 1
U2 4
PU HINDAWI LTD
PI LONDON
PA ADAM HOUSE, 3RD FLR, 1 FITZROY SQ, LONDON, WIT 5HE, ENGLAND
SN 1687-885X
EI 1687-8868
J9 INT J GEOPHYS
JI Int. J. Geophys.
PY 2016
AR 2410573
DI 10.1155/2016/2410573
PG 50
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DF0RI
UT WOS:000371046200001
ER
PT J
AU Gary, SP
Jian, LK
Broiles, TW
Stevens, ML
Podesta, JJ
Kasper, JC
AF Gary, S. Peter
Jian, Lan K.
Broiles, Thomas W.
Stevens, Michael L.
Podesta, John J.
Kasper, Justin C.
TI Ion-driven instabilities in the solar wind: Wind observations of 19
March 2005
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind; instabilities
ID PROTON TEMPERATURE ANISOTROPY; ELECTROMAGNETIC INSTABILITIES;
MAGNETOSONIC INSTABILITY; CYCLOTRON WAVES; PLASMA; BEAM; CONSTRAINT;
SPACECRAFT; STABILITY; STREAMS
AB Intervals of enhanced magnetic fluctuations have been frequently observed in the solar wind. But it remains an open question as to whether these waves are generated at the Sun and then transported outward by the solar wind or generated locally in the interplanetary medium. Magnetic field and plasma measurements from the Wind spacecraft under slow solar wind conditions on 19 March 2005 demonstrate seven events of enhanced magnetic fluctuations at spacecraft-frame frequencies somewhat above the proton cyclotron frequency and propagation approximately parallel or antiparallel to the background magnetic field B-o. The proton velocity distributions during these events are characterized by two components: a more dense, slower core and a less dense, faster beam. Observed plasma parameters are used in a kinetic linear dispersion equation analysis for electromagnetic fluctuations at k x B-o=0; for two events the most unstable mode is the Alfven-cyclotron instability driven by a proton component temperature anisotropy T/T-||>1 (where the subscripts denote directions relative to B-o), and for three events the most unstable mode is the right-hand polarized magnetosonic instability driven primarily by ion component relative flows. Thus, both types of ion anisotropies and both types of instabilities are likely to be local sources of these enhanced fluctuation events in the solar wind.
C1 [Gary, S. Peter; Podesta, John J.] Space Sci Inst, Boulder, CO USA.
[Jian, Lan K.] Univ Maryland, Goddard Planetary Heliophys Inst, College Pk, MD 20742 USA.
[Jian, Lan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Broiles, Thomas W.] Southwest Res Inst, San Antonio, TX USA.
[Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kasper, Justin C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Gary, SP (reprint author), Space Sci Inst, Boulder, CO USA.
EM pgary@lanl.gov
RI Jian, Lan/B-4053-2010;
OI Jian, Lan/0000-0002-6849-5527; Broiles, Thomas/0000-0001-6910-2724
FU NASA [NNX15AB75G, NNX13AI65G]
FX The research efforts of S.P.G., L.K.J., and T.W.B. were supported by the
NASA Living with a Star project NNX15AB75G entitled "Understanding
Wave-Particle Interactions between Solar Wind Plasma Waves and Heavy
Ions." L.K.J.'s work was also supported by NASA award NNX13AI65G. The
observational data for magnetic fields used herein are available at NASA
National Space Science Data Center (NSSDC). The observations of plasma
parameters are available from Michael Stevens, and the dispersion
relations computed from linear theory are available from S. Peter Gary.
NR 40
TC 7
Z9 7
U1 2
U2 2
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 JAN
PY 2016
VL 121
IS 1
BP 30
EP 41
DI 10.1002/2015JA021935
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900003
PM 27818854
ER
PT J
AU Glocer, A
Dorelli, J
Toth, G
Komar, CM
Cassak, PA
AF Glocer, A.
Dorelli, J.
Toth, G.
Komar, C. M.
Cassak, P. A.
TI Separator reconnection at the magnetopause for predominantly northward
and southward IMF: Techniques and results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; reconnection; flux transfer event; numerical modeling;
resistive MHD
ID GENERAL MAGNETIC RECONNECTION; FLUX-TRANSFER EVENTS; FIELD;
MAGNETOHYDRODYNAMICS; MAGNETOSPHERE; SIMULATIONS; TOPOLOGY; PHYSICS;
NULLS
AB In this work, we demonstrate how to track magnetic separators in three-dimensional simulated magnetic fields with or without magnetic nulls, apply these techniques to enhance our understanding of reconnection at the magnetopause. We present three methods for locating magnetic separators and apply them to 3-D resistive MHD simulations of the Earth's magnetosphere using the Block-Adaptive-Tree Solar-wind Roe-type Upwind Scheme code. The techniques for finding separators and determining the reconnection rate are insensitive to interplanetary magnetic field (IMF) clock angle and can in principle be applied to any magnetospheric model. Moreover, the techniques have a number of advantages over prior separator finding techniques applied to the magnetosphere. The present work examines cases of high and low resistivity for two clock angles. We go beyond previous work examine the separator during Flux Transfer Events (FTEs). Our analysis of reconnection on the magnetopause yields a number of interesting conclusions: Reconnection occurs all along the separator even during predominately northward IMF cases. Multiple separators form in low-resistivity conditions, and in the region of an FTE the separator splits into distinct branches. Moreover, the local contribution to the reconnection rate, as determined by the local parallel electric field, drops in the vicinity of the FTE with respect to the value when there are none.
C1 [Glocer, A.; Dorelli, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Toth, G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Komar, C. M.; Cassak, P. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM alex.glocer-1@nasa.gov
RI Toth, Gabor/B-7977-2013
OI Toth, Gabor/0000-0002-5654-9823
FU NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center; NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center; NASA Geospace
SRT project; NSF [AGS-0953463]
FX Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center and the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. A. Glocer effort was
supported by a project through the NASA Living With A Star program and
J. Dorrelli was supported by a NASA Geospace SR&T project. P.A. Cassak
was supported by NSF grant AGS-0953463. The tool used to locate
separators will be made available through the Community Coordinated
Modeling Center (CCMC), and the BATS-R-US code used to run the numerical
simulations is available through the University of Michigan for
download.
NR 34
TC 4
Z9 4
U1 0
U2 3
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 JAN
PY 2016
VL 121
IS 1
BP 140
EP 156
DI 10.1002/2015JA021417
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900011
ER
PT J
AU Stephens, GK
Sitnov, MI
Ukhorskiy, AY
Roelof, EC
Tsyganenko, NA
Le, G
AF Stephens, G. K.
Sitnov, M. I.
Ukhorskiy, A. Y.
Roelof, E. C.
Tsyganenko, N. A.
Le, G.
TI Empirical modeling of the storm time innermost magnetosphere using Van
Allen Probes and THEMIS data: Eastward and banana currents
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE empirical geomagnetic field; ring current; eastward current; magnetic
storm
ID DAWN-DUSK ASYMMETRY; RING CURRENT; PLASMA PRESSURE; GEOMAGNETIC STORMS;
CONVECTION EVENTS; MAGNETIC-FIELD; SIMULATION; DECAY
AB The structure of storm time currents in the inner magnetosphere, including its innermost region inside 4R(E), is studied for the first time using a modification of the empirical geomagnetic field model TS07D and new data from Van Allen Probes and Time History of Events and Macroscale Interactions during Substorms missions. It is shown that the model, which uses basis-function expansions instead of ad hoc current modules to approximate the magnetic field, consistently improves its resolution and magnetic field reconstruction with the increase of the number of basis functions and resolves the spatial structure and evolution of the innermost eastward current. This includes a connection between the westward ring current flowing largely at R greater than or similar to 3R(E) and the eastward ring current concentrated at R greater than or similar to 3R(E) resulting in a vortex current pattern. A similar pattern coined banana current' was previously inferred from the pressure distributions based on the energetic neutral atom imaging and first-principles ring current simulations. The morphology of the equatorial currents is dependent on storm phase. During the main phase, it is complex, with several asymmetries forming banana currents. Near SYM-H minimum, the banana current is strongest, is localized in the evening-midnight sector, and is more structured compared to the main phase. It then weakens during the recovery phase resulting in the equatorial currents to become mostly azimuthally symmetric.
C1 [Stephens, G. K.; Sitnov, M. I.; Ukhorskiy, A. Y.; Roelof, E. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Tsyganenko, N. A.] St Petersburg State Univ, Inst & Fac Phys, St Petersburg 199034, Russia.
[Le, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Stephens, GK (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM Grant.Stephens@jhuapl.edu
RI Ukhorskiy, Aleksandr/E-6429-2016; Sitnov, Mikhail/H-2316-2016; Le,
Guan/C-9524-2012;
OI Ukhorskiy, Aleksandr/0000-0002-3326-4024; Le, Guan/0000-0002-9504-5214;
Tsyganenko, Nikolai/0000-0002-5938-1579
FU NSF [AGS-1157463/115366]; Advanced Simulation and Computing Program;
Scientific Discovery through Advanced Computing Program
FX The authors thank B. H. Mauk for useful discussions. This work was
supported by the NSF grant AGS-1157463/115366. The magnetospheric data
were obtained from the public archive at NASA/GSFC Space Physics Data
Facility via their CDAWEB ftp site of CDF files
(ftp://cdaweb.gsfc.nasa.gov/). Solar wind and IMF data were obtained
from the OMNI database (http://omniweb.gsfc.nasa.gov/ow_min.html). The
OMNI data files include the Sym-H index that is offered by the World
Data Center for Geomagnetism of Kyoto University. We thank the AMPERE
team and the AMPERE Science Center for providing the Iridium derived
data products. The 3-D visualizations were performed using VisIt, which
is supported by the Department of Energy with funding from the Advanced
Simulation and Computing Program and the Scientific Discovery through
Advanced Computing Program. The data used to produce figures and
analysis in the paper are available upon request.
NR 41
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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 JAN
PY 2016
VL 121
IS 1
BP 157
EP 170
DI 10.1002/2015JA021700
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900012
ER
PT J
AU He, F
Zhang, XX
Chen, B
Fok, MC
Nakano, S
AF He, Fei
Zhang, Xiao-Xin
Chen, Bo
Fok, Mei-Ching
Nakano, Shinya
TI Determination of the Earth's plasmapause location from the CE-3 EUVC
images
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE plasmasphere; plasmapause; EUV imaging; Chang'e-3; reconstruction
ID EXTREME-ULTRAVIOLET IMAGER; ELECTRIC-FIELD; SATELLITE-OBSERVATIONS;
PLASMASPHERE; DENSITY; CAMERA; THEMIS; MODEL; MOON; CALIBRATION
AB The Moon-based Extreme Ultraviolet Camera (EUVC) aboard China's Chang'e-3 (CE-3) mission has successfully imaged the entire Earth's plasmasphere for the first time from the side views on lunar surface. An EUVC image on 21 April 2014 is used in this study to demonstrate the characteristics and configurations of the Moon-based EUV imaging and to illustrate the determination algorithm of the plasmapause locations on the magnetic equator. The plasmapause locations determined from all the available EUVC images with the Minimum L Algorithm are quantitatively compared with those extracted from in situ observations (Defense Meteorological Satellite Program, Time History of Events and Macroscale Interactions during Substorms, and Radiation Belt Storm Probes). Excellent agreement between the determined plasmapauses seen by EUVC and the extracted ones from other satellites indicates the reliability of the Moon-based EUVC images as well as the determination algorithm. This preliminary study provides an important basis for future investigation of the dynamics of the plasmasphere with the Moon-based EUVC imaging.
C1 [He, Fei; Chen, Bo] Chinese Acad Sci, Changchun Inst Opt Fine Mech & Phys, Changchun, Peoples R China.
[Zhang, Xiao-Xin] China Meteorol Adm, Natl Ctr Space Weather, Key Lab Space Weather, Beijing, Peoples R China.
[Fok, Mei-Ching] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Nakano, Shinya] Inst Stat Math, Tachikawa, Tokyo, Japan.
RP Zhang, XX (reprint author), China Meteorol Adm, Natl Ctr Space Weather, Key Lab Space Weather, Beijing, Peoples R China.
EM xxzhang@cma.gov.cn
OI Zhang, XiaoXin/0000-0002-7759-7402; HE, Fei/0000-0003-0542-2686; Nakano,
Shin'ya/0000-0003-0772-4610
FU Chinese Academy of Sciences [KGZD-EW-603]; National Natural Science
Foundation of China [41204102, 41274147]; National Basic Research
Program of China [2012CB957800, 2011CB811400]; National Hi-Tech Research
and Development Program of China [2012AA121000]
FX The authors sincerely thank the valuable discussions with the members of
the EUVC scientific team, especially Hua-Ning Wang, Jing-Song Ping, Chao
Shen, and Yong-Liao Zou. The authors are grateful to the National
Astronomical Observatories, Chinese Academy of Sciences, for the
provision of the CE-3 EUVC data. The authors also thank
NOAA/NESDIS/National Geophysical Data Center for the provision of the
DMSP data available from http:// satdat.ngdc.noaa.gov/dmsp/data/, Iowa
University for the provision of the EMFISIS data available from
http://emfisis.physics.uiowa.edu/data/index, and the THEMIS team for
provision of the THEMIS data available from
http://themis.ssl.berkeley.edu/index.shtml. The authors give thanks to
NASA-CCMC for providing the code of IGRF and Tsyganenko model. This work
was supported by the Key Research Project of Chinese Academy of
Sciences: Application research on the scientific data from Chang'E-3
mission (KGZD-EW-603), the National Natural Science Foundation of China
(41204102 and 41274147), the National Basic Research Program of China
(2012CB957800 and 2011CB811400), and the National Hi-Tech Research and
Development Program of China (2012AA121000).
NR 41
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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 JAN
PY 2016
VL 121
IS 1
BP 296
EP 304
DI 10.1002/2015JA021863
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900022
ER
PT J
AU Lee, SH
Zhang, H
Zong, QG
Otto, A
Reme, H
Liebert, E
AF Lee, S. H.
Zhang, H.
Zong, Q. -G.
Otto, A.
Reme, H.
Liebert, E.
TI A statistical study of plasmaspheric plumes and ionospheric outflows
observed at the dayside magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE plasmaspheric plume; ionospheric outflow; dayside magnetopause;
statistical study
ID INTERPLANETARY MAGNETIC-FIELD; PITCH-ANGLE DISTRIBUTIONS; SOLAR MINIMUM
CONDITIONS; IN-SITU OBSERVATIONS; ALTITUDE POLAR-CAP; ION OUTFLOW;
ELECTRIC-FIELD; MAGNETOSPHERIC CONVECTION; EARTHS MAGNETOSPHERE; OUTER
MAGNETOSPHERE
AB We present a statistical study of plasmaspheric plumes and ionospheric outflows observed by the Cluster spacecraft near the dayside magnetopause. Plasmaspheric plumes are identified when the low-energy ions (<1keV) with approximate to 90 degrees pitch angle distributions are observed by the Cluster Ion Spectrometer/Hot Ion Analyzer instrument. The ionospheric outflows are characterized by unidirectional or bidirectional field-aligned pitch angle distributions of low-energy ions observed in the dayside magnetosphere. Forty-three (10%) plasmaspheric plume events and 32 (7%) ionospheric outflow events were detected out of the 442 times that C3 crossed the dayside magnetopause between 2007 and 2009. The occurrence rate of plumes at duskside is significantly higher than that at dawnside. The occurrence rate of outflows shows a weak dawn-dusk asymmetry. We investigate the dependence of the occurrence rates of plumes and ionospheric outflows on geomagnetic activity and on solar wind/interplanetary magnetic field (IMF) conditions. The plume events tend to occur during southward IMF (duskward solar wind electric field) and moderate geomagnetic activity (Kp = 3,-30Dst <- 10nT). However, the ionospheric outflow events tend to occur during northward IMF (dawnward solar wind electric field). The ionospheric outflows do not occur when Kp = 0, and the occurrence rate of the ionospheric outflows does not have a clear Dst dependence. Seventy-five percent (46%) of the outflows are observed in the duskside for negative (positive) IMF B-y. Conversely, 54% (25%) of the outflows are observed in the dawnside for positive (negative) IMF B-y. Finally, the occurrence rates of both plumes and outflows increase with solar wind dynamic pressure.
C1 [Lee, S. H.; Zhang, H.; Otto, A.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Lee, S. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Zong, Q. -G.] Peking Univ, Sch Earth & Space Sci, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China.
[Reme, H.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Reme, H.] CNRS, IRAP, Toulouse, France.
[Liebert, E.] Inst Geophys & Extraterr Phys, Braunschweig, Germany.
RP Zhang, H (reprint author), Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
EM hzhang14@alaska.edu
FU NSF [AGS-1007449]; National Natural Science Foundation of China
[41421003]; Chinese National Programs for Fundamental Research and
Development [2012CB825603]; Deutsches Zentrum fur Luft- und Raumfahrt
[50 OC1402]
FX We thank the instrument teams of Cluster mission and ESA Cluster Science
Archive for the successful spacecraft operation and for providing plasma
and magnetic field data (http://www.cosmos.esa.int/web/csa). The Kp and
Dst indices were provided by the website
(http://wdc.kugi.kyoto-u.ac.jp/). The IMF and the derived solar wind
electric field, Ey, were provided by the OMNIWeb
(http://omniweb.gsfc.nasa.gov/). H. Zhang was supported by NSF grant
AGS-1007449. Q.-G. Zong was supported by National Natural Science
Foundation of China (41421003) and Major Project of Chinese National
Programs for Fundamental Research and Development (2012CB825603). E.
Liebert was financially supported through grant 50 OC1402 by the
Deutsches Zentrum fur Luft- und Raumfahrt.
NR 71
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U1 1
U2 3
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 JAN
PY 2016
VL 121
IS 1
BP 492
EP 506
DI 10.1002/2015JA021540
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900035
ER
PT J
AU Cessateur, G
De Keyser, J
Maggiolo, R
Gibbons, A
Gronoff, G
Gunell, H
Dhooghe, F
Loreau, J
Vaeck, N
Altwegg, K
Bieler, A
Briois, C
Calmonte, U
Combi, MR
Fiethe, B
Fuselier, SA
Gombosi, TI
Hassig, M
Le Roy, L
Neefs, E
Rubin, M
Semon, T
AF Cessateur, G.
De Keyser, J.
Maggiolo, R.
Gibbons, A.
Gronoff, G.
Gunell, H.
Dhooghe, F.
Loreau, J.
Vaeck, N.
Altwegg, K.
Bieler, A.
Briois, C.
Calmonte, U.
Combi, M. R.
Fiethe, B.
Fuselier, S. A.
Gombosi, T. I.
Haessig, M.
Le Roy, L.
Neefs, E.
Rubin, M.
Semon, T.
TI Photochemistry of forbidden oxygen lines in the inner coma of
67P/Churyumov-Gerasimenko
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ROSINA; DFMS; 67P; Churyumov-Gerasimenko; oxygen line emissions; airglow
ID ATOMIC OXYGEN; HALE-BOPP; SOLAR; PHOTODISSOCIATION; MISSION; COMETS; ION
AB Observations of the green and red-doublet emission lines have previously been realized for several comets. We present here a chemistry-emission coupled model to study the production and loss mechanisms of the O(S-1) and O(D-1) states, which are responsible for the emission lines of interest for comet 67P/Churyumov-Gerasimenko. The recent discovery of O-2 in significant abundance relative to water 3.800.85 within the coma of 67P has been taken into consideration for the first time in such models. We evaluate the effect of the presence of O-2 on the green to red-doublet emission intensity ratio, which is traditionally used to assess the CO2 abundance within cometary atmospheres. Model simulations, solving the continuity equation with transport, show that not taking O-2 into account leads to an underestimation of the CO2 abundance within 67P, with a relative error of about 25%. This strongly suggests that the green to red-doublet emission intensity ratio alone is not a proper tool for determining the CO2 abundance, as previously suggested. Indeed, there is no compelling reason why O-2 would not be a common cometary volatile, making revision of earlier assessments regarding the CO2 abundance in cometary atmospheres necessary. The large uncertainties of the CO2 photodissociation cross section imply that more studies are required in order to better constrain the O(S-1) and O(D-1) production through this mechanism. Space weather phenomena, such as powerful solar flares, could be used as tools for doing so, providing additional information on a good estimation of the O-2 abundance within cometary atmospheres.
C1 [Cessateur, G.; De Keyser, J.; Maggiolo, R.; Gibbons, A.; Gunell, H.; Dhooghe, F.] Royal Belgian Inst Space Aeron, Space Phys Div, Brussels, Belgium.
[De Keyser, J.] Katholieke Univ Leuven, Ctr Plasma Astrophys, B-3001 Heverlee, Belgium.
[Gibbons, A.; Loreau, J.; Vaeck, N.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, Brussels, Belgium.
[Gronoff, G.] NASA, Langley Res Ctr, Chem & Dynam Branch, Sci Directorate, Hampton, VA 23665 USA.
[Gronoff, G.] SSAI, Hampton, VA USA.
[Altwegg, K.; Bieler, A.; Calmonte, U.; Haessig, M.; Le Roy, L.; Rubin, M.; Semon, T.] Univ Bern, Inst Phys, Bern, Switzerland.
[Altwegg, K.] Univ Bern, Ctr Space & Habitabil, Bern, Switzerland.
[Bieler, A.; Combi, M. R.; Gombosi, T. I.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Briois, C.] Univ Orleans, Lab Phys & Chim Envirom & Espace, UMR CNRS 7328, Orleans, France.
[Fiethe, B.] TU Braunschweig, Inst Comp & Network Engn IDA, Braunschweig, Germany.
[Fuselier, S. A.; Haessig, M.] SW Res Inst, Div Space Sci, San Antonio, TX USA.
[Fuselier, S. A.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Neefs, E.] Royal Belgian Inst Space Aeron, Div Engn, Brussels, Belgium.
RP Cessateur, G (reprint author), Royal Belgian Inst Space Aeron, Space Phys Div, Brussels, Belgium.
EM gael.cessateur@aeronomie.be
RI Combi, Michael/J-1697-2012; Gombosi, Tamas/G-4238-2011; Rubin,
Martin/I-7777-2013;
OI Combi, Michael/0000-0002-9805-0078; Gombosi, Tamas/0000-0001-9360-4951;
Rubin, Martin/0000-0001-6549-3318; Gronoff,
Guillaume/0000-0002-0331-7076; Dhooghe, Frederik/0000-0001-7334-833X
FU Fonds de la Recherche Scientifique [PDR T.1073.14]; Belgian Science
Policy Office [PRODEX/ROSINAPEA4000107705]; Belgian Fund for Scientific
Research - FNRS; State of Bern; Swiss National Science Foundation;
European Space Agency PRODEX Program; Jet Propulsion Laboratory
[1496541]; NASA [JPL-1266313]; NASA Astrobiology Institute [NNX15AE05G];
NASA HIDEE program; [2014-12-19)]; [P7/15]
FX Work at BIRA-IASB was supported by the Fonds de la Recherche
Scientifique grant PDR T.1073.14 comparative study of atmospheric
erosion, by the Belgian Science Policy Office via
PRODEX/ROSINAPEA4000107705 and an Additional Researchers grant
(Ministerial Decree of 2014-12-19), and by the Interuniversitary
Attraction Pole P7/15 "Planets: tracing the Transfer, Origin,
Preservation and Evolution of their Reservoirs". Work at the ULB was
supported by the Belgian Fund for Scientific Research - FNRS. Work at
UoB was funded by the State of Bern, the Swiss National Science
Foundation, and by the European Space Agency PRODEX Program. Work at
Southwest Research Institute was supported by subcontract 1496541 from
the Jet Propulsion Laboratory. Work at the University of Michigan was
funded by NASA under contract JPL-1266313. G.G. was supported by NASA
Astrobiology Institute grant NNX15AE05G and by the NASA HIDEE program.
Rosetta is an ESA mission with contributions from its member states and
NASA. The results from Rosetta and ROSINA would not be possible without
the work of the many engineers, technicians, and scientists involved in
the mission over the past 20 years, whose contributions are gratefully
acknowledged. All Rosetta/ROSINA data are available on request until
they are released to the PSA archive of ESA (www.rssd.esa.int/PSA) and
to the PDS archive of NASA. The solar UV flux data were obtained from
the LISIRD database (http://lasp.colorado.edu/lisird/ssi/). The
cross-sections data used in this paper can be obtained from the
PHIDRATES database (http://phidrates.space.swri.edu/), and from the
ATMOCIAD database which is available from the authors upon request
(Guillaume. P.Gronoff@nasa.gov). The authors would like to thank the
anonymous reviewers for their insightful comments and suggestions that
have contributed to improve this paper.
NR 37
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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 JAN
PY 2016
VL 121
IS 1
BP 804
EP 816
DI 10.1002/2015JA022013
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900058
ER
PT J
AU Park, J
Martinis, CR
Luhr, H
Pfaff, RF
Kwak, YS
AF Park, Jaeheung
Martinis, Carlos R.
Luehr, Hermann
Pfaff, Robert F.
Kwak, Young-Sil
TI Hemispheric asymmetry in transition from equatorial plasma bubble to
blob as deduced from 630.0nm airglow observations at low latitudes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE low-latitude blob; hemispheric conjugacy; equatorial plasma bubble
ID SWARM CONSTELLATION; HINOTORI SATELLITE; IMPEDANCE PROBE; SPREAD-F;
ENHANCEMENTS; MIDLATITUDE; IONOSPHERE; BOARD
AB Transitions from depletions to enhancements of 630.0nm nighttime airglow have been observed at Arecibo. Numerical simulations by Krall et al. (2009) predicted that they should occur only in one hemisphere, which has not yet been confirmed observationally. In this study we investigate the hemispheric conjugacy of the depletion-to-enhancement transition using multiple instruments. We focus on one event observed in the American longitude sector on 22 December 2014: 630.0nm airglow depletions evolved into enhancements in the Northern Hemisphere while the evolution did not occur in the conjugate location in the Southern Hemisphere. Concurrent plasma density measured by low Earth orbit (LEO) satellites and 777.4nm airglow images support that the depletions and enhancements of 630.0nm nighttime airglow reflect plasma density decreases and increases (blobs), respectively. Characteristics of the airglow depletions, in the context of the LEO satellite data, further suggest that the plasma density depletion deduced from the airglow data represents equatorial plasma bubbles (EPBs) rather than medium-scale traveling ionospheric disturbances from midlatitudes. Hence, the event in this study can be interpreted as EPB-to-blob transition.
C1 [Park, Jaeheung; Kwak, Young-Sil] Korea Astron & Space Sci Inst, Daejeon, South Korea.
[Park, Jaeheung; Kwak, Young-Sil] Univ Sci & Technol, Dept Astron & Space Sci, Daejeon, South Korea.
[Martinis, Carlos R.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Luehr, Hermann] Helmholtz Ctr Potsdam, GFZ German Res Ctr Geosci, Potsdam, Germany.
[Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Park, J (reprint author), Korea Astron & Space Sci Inst, Daejeon, South Korea.; Park, J (reprint author), Univ Sci & Technol, Dept Astron & Space Sci, Daejeon, South Korea.
EM pj@kasi.re.kr
FU "Planetary system research for space exploration" project from KASI; Air
Force Research Laboratory [FA2386-14-1-4004]; NSF [1123222]; Office of
Naval Research
FX The European Space Agency (ESA) is acknowledged for providing the Swarm
data. The Swarm Level-1b data are accessible if one follows the method
described at https://earth.esa.int/web/guest/swarm/data-access. We would
like to thank the personnel involved in the DMSP data service at
http://satdat.ngdc.noaa.gov/dmsp/. The Communication/Navigation Outage
Forecast System (C/NOFS) mission, conceived and developed by the Air
Force Research Laboratory, is sponsored and executed by the USAF Space
Test Program. The OMNI data were obtained from the GSFC/SPDF OMNIWeb
interface at http://omniweb.gsfc.nasa.gov. Raw all-sky airglow images
are available at http://www.buimaging.com. All data used for this study
are available by contacting J. Park (pj@kasi.re.kr). J. Park was
partially supported by the "Planetary system research for space
exploration" project, the basic research funding from KASI, and the Air
Force Research Laboratory, under agreement FA2386-14-1-4004. C.M.
acknowledges the support of NSF grant 1123222 and Office of Naval
Research grant.
NR 29
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U1 3
U2 4
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 JAN
PY 2016
VL 121
IS 1
BP 881
EP 893
DI 10.1002/2015JA022175
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF2CJ
UT WOS:000371146900064
ER
PT J
AU Tiano, AL
Gibbons, L
Tsui, M
Applin, SI
Silva, R
Park, C
Fay, CC
AF Tiano, A. L.
Gibbons, L.
Tsui, M.
Applin, S. I.
Silva, R.
Park, C.
Fay, C. C.
TI Thermodynamic approach to boron nitride nanotube solubility and
dispersion
SO NANOSCALE
LA English
DT Article
ID WALLED CARBON NANOTUBES; SOLVENT MIXTURES; FUNCTIONALIZATION;
PARAMETERS; GROWTH; ROPES; WATER
AB Inadequate dispersion of nanomaterials is a critical issue that significantly limits the potential properties of nanocomposites and when overcome, will enable further enhancement of material properties. The most common methods used to improve dispersion include surface functionalization, surfactants, polymer wrapping, and sonication. Although these approaches have proven effective, they often achieve dispersion by altering the surface or structure of the nanomaterial and ultimately, their intrinsic properties. Co-solvents are commonly utilized in the polymer, paint, and art conservation industries to selectively dissolve materials. These co-solvents are utilized based on thermodynamic interaction parameters and are chosen so that the original materials are not affected. The same concept was applied to enhance the dispersion of boron nitride nanotubes (BNNTs) to facilitate the fabrication of BNNT nanocomposites. Of the solvents tested, dimethylacetamide (DMAc) exhibited the most stable, uniform dispersion of BNNTs, followed by N, N-dimethylformamide (DMF), acetone, and N-methyl-2-pyrrolidone (NMP). Utilizing the known Hansen solubility parameters of these solvents in comparison to the BNNT dispersion state, a region of good solubility was proposed. This solubility region was used to identify co-solvent systems that led to improved BNNT dispersion in poor solvents such as toluene, hexane, and ethanol. Incorporating the data from the co-solvent studies further refined the proposed solubility region. From this region, the Hansen solubility parameters for BNNTs are thought to lie at the midpoint of the solubility sphere: 16.8, 10.7, and 9.0 MPa1/2 for delta(d), delta(p), and delta(h), respectively, with a calculated Hildebrand parameter of 21.8 MPa1/2.
C1 [Tiano, A. L.; Gibbons, L.; Applin, S. I.] Natl Inst Aerosp, 100 Exploration Way, Hampton, VA 23666 USA.
[Tsui, M.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Silva, R.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Park, C.; Fay, C. C.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Park, C (reprint author), NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
EM cheol.park-1@nasa.gov
FU NASA; US Air Force Office of Scientific Research - Low Density Materials
program [FA9550-11-1-0042]; NASA Langley Research Center Undergraduate
Research Program (USRP)
FX This work was supported in part by the NASA Langley Creativity and
Innovation, Internal Research and Development, and Bid and Proposal
programs, as well as the NASA Game Changing Development Seedling
programs. C. Park acknowledges funding in part by the US Air Force
Office of Scientific Research - Low Density Materials program under
Grant No. FA9550-11-1-0042. The authors also thank the Langley Aerospace
Research Summer Scholars (LARSS) and the NASA Langley Research Center
Undergraduate Research Program (USRP) for their sponsorship of R. Silva
and M. Tsui. The authors would also like to thank Dr Sang-Hyon Chu and
Dr Siviram Arepalli for fruitful discussions and helpful comments on
this work. C. Park also thanks Dr W. Cao for HRTEM imaging of BNNTs.
NR 49
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U2 38
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2040-3364
EI 2040-3372
J9 NANOSCALE
JI Nanoscale
PY 2016
VL 8
IS 7
BP 4348
EP 4359
DI 10.1039/c5nr08259e
PG 12
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA DE6RQ
UT WOS:000370761700057
PM 26839175
ER
PT J
AU Shofners, GA
Campbell, AJ
Danielson, LR
Righter, K
Fischer, RA
Wang, YB
Prakapenka, V
AF Shofners, Gregory A.
Campbell, Andrew J.
Danielson, Lisa R.
Righter, Kevin
Fischer, Rebecca A.
Wang, Yanbin
Prakapenka, Vitali
TI The W-WO2 oxygen fugacity buffer (WWO) at high pressure and temperature:
Implications for f(o2) buffering and metal-silicate partitioning
SO AMERICAN MINERALOGIST
LA English
DT Article
DE High pressure; tungsten; oxygen fugacity buffer; equation of state;
metal-silicate partitioning
ID MULTI-ANVIL EXPERIMENTS; X-RAY-DIFFRACTION; EQUATION-OF-STATE; CORE
FORMATION; SIDEROPHILE ELEMENTS; TUNGSTEN; MOLYBDENUM; LIQUID; SYSTEM;
CONSTRAINTS
AB Synchrotron X-ray diffraction data were obtained to simultaneously measure unit-cell volumes of W and WO2 at pressures and temperatures up to 70 GPa and 2300 K. Both W and WO2 unit-cell volume data were fit to Mie-Gruneisen equations of state; parameters for W are Kr = 307 ( 0.4) GPa, K-T = 4.05 (+/- 0.04), yo = 1.61 ( 0.03), and q = 1.54 ( 0.13). Three phases were observed in WO2 with structures in the P2(1)/c, Pnma, and C2c space groups. The transition pressures are 4 and 32 GPa for the P211 c-Pnma and Pnma-C2I c phase changes, respectively. The P2,/c and Pnma phases have previously been described, whereas the C2I c phase is newly described here. Equations of state were fitted for these phases over their respective pressure ranges yielding the parameters KT = 238 ( 7), 230 ( 5), 304 ( 3) GPa, K-j, = 4 (fixed), 4 (fixed), 4 (fixed) GPa, yo = 1.45 (+/- 0.18), 1.22 ( 0.07), 1.21 ( 0.12), and q =1 (fixed), 2.90 (+/- 1.5), 1 (fixed) for the P2(1)/c, Pnma, and C2I c phases, respectively. The W-W02 buffer (WWO) was extended to high pressure using these W and WO2 equations of state. The T-f02 slope of the WWO buffer along isobars is positive from 1000 to 2500 K with increasing pressure up to at least 60 GPa. The WWO buffer is at a higher foe than the iron-wilstite (IW) buffer at pressures lower than 40 GPa, and the magnitude of this difference decreases at higher pressures. This implies an increasingly lithophile character for W at higher pressures. The WWO buffer was quantitatively applied to W metal-silicate partitioning by using the WWO-IW buffer difference in combination with literature data on W metal-silicate partitioning to model the exchange coefficient (KE,) for the Fe-W exchange reaction. This approach captures the non-linear pressure dependence of W metal-silicate partitioning using the W WO-IW buffer difference. Calculation of KD along a peridotite liquidus predicts a decrease in W siderophility at higher pressures that supports the qualitative behavior predicted by the WWO-IVV buffer difference, and agrees with findings of others. Comparing the competing effects of temperature and pressure the results here indicate that pressure exerts a greater effect on W metal-silicate partitioning.
C1 [Shofners, Gregory A.] Towson Univ, Dept Phys Astron & Geosci, 8000 York Rd, Towson, MD 21252 USA.
[Campbell, Andrew J.; Fischer, Rebecca A.] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
[Danielson, Lisa R.] NASA, Jacobs Technol, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Righter, Kevin] NASA, Johnson Space Ctr, 2101 NASA Pkwy,Mailcode XI2, Houston, TX 77058 USA.
[Wang, Yanbin; Prakapenka, Vitali] Univ Chicago, Ctr Adv Radiat Sources, Argonne Natl Lab, 9700 South Cass Ave,Bldg 434A, Argonne, IL 60439 USA.
RP Shofners, GA (reprint author), Towson Univ, Dept Phys Astron & Geosci, 8000 York Rd, Towson, MD 21252 USA.
EM gshofner@towson.edu
FU NASA GSRP fellowship; NASA RTOP from the Cosmochemistry program; NSF
[EAR-1243847]; NSF GSFP; University of Maryland; National Science
Foundation, Earth Sciences [EAR-1128799]; Department of
Energy-GeoSciences [DE-FG02-94ER14466]; DOE Office of Science by Argonne
National Laboratory [DE-AC02-06CH11357]
FX This research was supported by a NASA GSRP fellowship to G.A.S., NASA
RTOP from the Cosmochemistry program to K.R., and NSF grant EAR-1243847
to A.J.C. R.A.F. was supported by the NSF GSFP and a Flagship Fellowship
from University of Maryland. High-pressure multi-anvil assemblies were
produced by the COMPRES Infrastructure Development Project. Portions of
this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced
Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is
supported by the National Science Foundation, Earth Sciences
(EAR-1128799) and Department of Energy-GeoSciences (DE-FG02-94ER14466).
This research used resources of the Advanced Photon Source, a U.S.
Department of Energy (DOE) Office of Science User Facility operated for
the DOE Office of Science by Argonne National Laboratory under Contract
No. DE-AC02-06CH11357. Assistance with RHDAC experiments was provided by
undergraduate researcher James Deane. Reviews by D. Walker, C. Lesher,
and several anonymous reviewers helped improve the clarity of the
manuscript.
NR 41
TC 2
Z9 2
U1 1
U2 10
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD JAN-FEB
PY 2016
VL 101
IS 1-2
BP 211
EP 221
DI 10.2138/am-2016-5328
PG 11
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DD8YT
UT WOS:000370213500020
ER
PT J
AU Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Biland, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, E
Bretz, T
Carmona, E
Carosi, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Da Vela, P
Dazzi, E
De Angelis, A
De Caneva, G
De Lotto, B
Wilhelmi, ED
Mendez, CD
Di Pierro, E
Prester, DD
Dorner, D
Doro, M
Einecke, S
Glawion, DE
Elsaesser, D
Fernandez-Barral, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Godinovic, N
Munoz, AG
Gozzini, SR
Hanabata, Y
Hayashida, M
Herrera, J
Hirotani, K
Hoses, J
Hrupec, D
Hughes, G
Idec, W
Kellermann, H
Knoetig, ML
Kodani, K
Konno, Y
Krause, J
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lewandowska, N
Lindfors, E
Lombardi, S
Longo, E
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorenz, E
Makariev, M
Mallot, K
Maneva, G
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Munar-Adrover, P
Nakajima, D
Neustroev, V
Niedzwiecki, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Garcia, IR
Saito, T
Saito, K
Satalecka, K
Scalzotto, V
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, E
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Torres, DF
Toyama, T
Treves, A
Ward, J
Will, M
Zanin, R
AF Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
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, E.
Bretz, T.
Carmona, E.
Carosi, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, E.
De Angelis, A.
De Caneva, G.
De Lotto, B.
de Ona Wilhelmi, E.
Delgado Mendez, C.
Di Pierro, E.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Garcia Lopez, R. J.
Garczarczyk, M.
Garrido Terrats, D.
Gaug, M.
Godinovic, N.
Gonzalez Munoz, A.
Gozzini, S. R.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hirotani, K.
Hoses, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kellermann, H.
Knoetig, M. L.
Kodani, K.
Konno, Y.
Krause, J.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lewandowska, N.
Lindfors, E.
Lombardi, S.
Longo, E.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorenz, E.
Makariev, M.
Mallot, K.
Maneva, G.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Munar-Adrover, P.
Nakajima, D.
Neustroev, V.
Niedzwiecki, A.
Rosillo, M. Nevas
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Reinthal, R.
Rhode, W.
Ribo, M.
Rico, J.
Garcia, I. Rodriguez
Saito, T.
Saito, K.
Satalecka, K.
Scalzotto, V.
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, E.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Torres, D. F.
Toyama, T.
Treves, A.
Ward, J.
Will, M.
Zanin, R.
TI Teraelectronvolt pulsed emission from the Crab Pulsar detected by MAGIC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma rays: stars; pulsars: individual: Crab pulsar; stars: neutron
ID GAMMA-RAY PULSARS; HIGH-ENERGY EMISSION; OUTER GAP MODEL; MAJOR UPGRADE;
SLOT GAPS; TELESCOPE; RADIATION; SPECTRA; NEBULA; ACCELERATION
AB Aims. We investigate the extension of the very high-energy spectral tail of the Crab Pulsar at energies above 400 GeV.
Methods. We analyzed similar to 320 h of good-quality Crab data obtained with the MAGIC telescope from February 2007 to April 2014.
Results. We report the most energetic pulsed emission ever detected from the Crab Pulsar reaching up to 1.5 TeV. The pulse profile shows two narrow peaks synchronized with those measured in the GeV energy range. The spectra of the two peaks follow two different power-law functions from 70GeV up to 1.5 TeV and connect smoothly with the spectra measured above 10GeV by the Large Area Telescope (LAT) on board the Fermi satellite. When making a joint fit of the LAT and MAGIC data above 10 GeV the photon indices of the spectra differ by 0.5 +/- 0.1.
Conclusions. Using data from the MAGIC telescopes we measured the most energetic pulsed photons from a pulsar to date. Such TeV pulsed photons require a parent population of electrons with a Lorentz factor of at least 5x10(6). These results strongly suggest IC scattering off low-energy photons as the emission mechanism and a gamma-ray production region in the vicinity of the light cylinder.
C1 [Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Longo, E.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Longo, E.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, E.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, E.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, Via Laterina 8, 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; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Zagreb 10000, Croatia.
[Bangale, P.; Barres de Almeida, U.; Borracci, E.; Colin, P.; Dazzi, E.; Fruck, C.; Hoses, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Menzel, U.; Mirzoyan, R.; Noda, K.; Paneque, D.; Garcia, I. Rodriguez; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Rosillo, M. Nevas; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain.
[Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Tescaro, D.; Will, M.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; De Caneva, G.; Garczarczyk, M.; Gozzini, S. R.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Hughes, G.; Knoetig, M. L.; Prandini, E.] ETH, CH-8093 Zurich, Switzerland.
[Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Gonzalez Munoz, A.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Ward, J.] IFAE, Bellaterra 08193, Spain.
[Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain.
[de Ona Wilhelmi, E.] Inst Space Sci CSIC IEEC, Barcelona 08193, Spain.
[Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.] Univ Padua, I-35131 Padua, Italy.
[Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain.
[Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
[Galindo, D.; Marcote, B.; Munar-Adrover, P.; 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.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto, Japan.
[Hirotani, K.] ASIAA, POB 23-141, Taipei 10617, Taiwan.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Oulu 90014, Finland.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, Oulu 90014, Finland.
[Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, Sofia 1784, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, Barcelona 08193, Spain.
[Torres, D. F.] Inst Space Sci, Barcelona 08193, Spain.
[Treves, A.] Univ Insubria, I-22100 Como, Italy.
[Treves, A.] INFN Milano Bicocca, I-22100 Como, Italy.
[Barres de Almeida, U.] Ctr Brasileiro Pesquisas Fis CBPF MCTI, R Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Becerra Gonzalez, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Becerra Gonzalez, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Becerra Gonzalez, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Lindfors, E.; Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Persic, M.] INAF Trieste, Trieste, Italy.
[Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland.
RP Ansoldi, S (reprint author), Univ Udine, I-33100 Udine, Italy.
RI Lopez Moya, Marcos/L-2304-2014; Font, Lluis/L-4197-2014; Temnikov,
Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev,
Martin/M-2122-2016; Miranda, Jose Miguel/F-2913-2013; Delgado,
Carlos/K-7587-2014; Barrio, Juan/L-3227-2014; GAug, Markus/L-2340-2014;
Cortina, Juan/C-2783-2017; Poutanen, Juri/H-6651-2016; Contreras
Gonzalez, Jose Luis/K-7255-2014;
OI Lopez Moya, Marcos/0000-0002-8791-7908; Font, Lluis/0000-0003-2109-5961;
Temnikov, Petar/0000-0002-9559-3384; Miranda, Jose
Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Barrio,
Juan/0000-0002-0965-0259; GAug, Markus/0000-0001-8442-7877; Cortina,
Juan/0000-0003-4576-0452; Poutanen, Juri/0000-0002-0983-0049; Contreras
Gonzalez, Jose Luis/0000-0001-7282-2394; Doro,
Michele/0000-0001-9104-3214; Torres, Diego F./0000-0002-1522-9065; 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
FU German BMBF; MPG; Italian INFN; INAF; Swiss National Fund SNF; ERDF
under the Spanish MINECO [FPA2012-39502]; Japanese JSPS; MEXT; Centro de
Excelencia Severo Ochoa [SEV-2012-0234]; CPAN project of the Spanish
Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the
Spanish Consolider-Ingenio programme [CSD2009-00064]; Croatian Science
Foundation (HrZZ) [09/176]; University of Rijeka [13.12.1.3.02]; DFG
Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW
[745/N-HESS-MAGIC/2010/0]; Academy of Finland [268740]
FX We would like to thank the Instituto 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 (FPA2012-39502), 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 SFB823/C4 and
SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.
NR 46
TC 5
Z9 5
U1 5
U2 19
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 JAN
PY 2016
VL 585
AR A133
DI 10.1051/0004-6361/201526853
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300140
ER
PT J
AU Borovicka, J
Shrbeny, L
Kalenda, P
Loskutov, N
Brown, P
Spurny, P
Cooke, W
Blaauw, R
Moser, DE
Kingery, A
AF Borovicka, J.
Shrbeny, L.
Kalenda, P.
Loskutov, N.
Brown, P.
Spurny, P.
Cooke, W.
Blaauw, R.
Moser, D. E.
Kingery, A.
TI A catalog of video records of the 2013 Chelyabinsk superbolide
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE meteorites; meteors; meteoroids
ID AIRBURST
AB The Chelyabinsk superbolide of February 15, 2013, was caused by the atmospheric entry of a similar to 19 m asteroid with a kinetic energy of 500 kT TNT just south of the city of Chelyabinsk, Russia. It was a rare event; impacts of similar energy occur on the Earth only a few times per century. Impacts of this energy near such a large urban area are expected only a few times per 10 000 years. A number of video records obtained by casual eyewitnesses, dashboard cameras in cars, security, and traffic cameras were made publicly available by their authors on the Internet. These represent a rich repository for future scientific studies of this unique event. To aid researchers in the archival study of this airburst, we provide and document a catalog of 960 videos showing various aspects of the event. Among the video records are 400 distinct videos showing the bolide itself and 108 videos showing the illumination caused by the bolide. Other videos show the dust trail left in the atmosphere, the arrival of the blast wave on the ground, or the damage caused by the blast wave. As these video recordings have high scientific, historical, and archival value for future studies of this airburst, a systematic documentation and description of records is desirable. Many have already been used for scientific analyses. We give the exact locations where 715 videos were taken as well as details of the visible/audible phenomena in each video recording. An online version of the published catalog has been developed and will be regularly updated to provide a long-term database for investigators.
C1 [Borovicka, J.; Shrbeny, L.; Spurny, P.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
[Kalenda, P.] Acad Sci Czech Republic, Inst Rock Struct & Mech, V Holesovickach 41, Prague 18209 8, Czech Republic.
[Loskutov, N.] OOO RC PLINOR, Pushkinskaya 12, St Petersburg 196626, Russia.
[Brown, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cooke, W.] NASA, George C Marshall Space Flight Ctr, Space Environm Team, Meteoroid Environm Off, EV44, Huntsville, AL 35812 USA.
[Blaauw, R.] NASA, George C Marshall Space Flight Ctr, All Points Jacobs ESSSA Grp, Huntsville, AL 35812 USA.
[Moser, D. E.] NASA, George C Marshall Space Flight Ctr, Jacobs Jacobs ESSSA Grp, Huntsville, AL 35812 USA.
[Kingery, A.] NASA, George C Marshall Space Flight Ctr, Jacobs ESSSA Grp, ERC Inc, Huntsville, AL 35812 USA.
RP Borovicka, J; Shrbeny, L (reprint author), Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
EM jiri.borovicka@asu.cas.cz; lukas.shrbeny@asu.cas.cz
RI Borovicka, Jiri/F-4257-2014; Spurny, Pavel/G-9044-2014; Shrbeny,
Lukas/G-9040-2014
FU GACR [P209/11/1382]; Praemium Academiae of the Czech Academy of
Sciences; Czech institutional project [RVO:67985815]; NASA [NNX11AB76A]
FX We thank L. Kotkova and J. Kotek for programming the online database, H.
Zichova for inspecting many videos, O. Popova for an early exchange of
information on some videos, D. Castek for providing his video in full
resolution, and authors of all videos for uploading them on the
Internet. This work was supported by grant P209/11/1382 from GACR,
Praemium Academiae of the Czech Academy of Sciences, the Czech
institutional project RVO:67985815, and NASA co-operative agreement
NNX11AB76A.
NR 12
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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 JAN
PY 2016
VL 585
AR A90
DI 10.1051/0004-6361/201526680
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300097
ER
PT J
AU Gobrecht, D
Cherchneff, I
Sarangi, A
Plane, JMC
Bromley, ST
AF Gobrecht, D.
Cherchneff, I.
Sarangi, A.
Plane, J. M. C.
Bromley, S. T.
TI Dust formation in the oxygen-rich AGB star IK Tauri
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: AGB and post-AGB; dust, extinction; stars: late-type; stars:
low-mass; astrochemistry; molecular processes
ID GIANT BRANCH STARS; VY-CANIS-MAJORIS; CIRCUMSTELLAR ENVELOPES;
HERSCHEL/HIFI OBSERVATIONS; MAGELLANIC-CLOUD; MIRA VARIABLES; INNER
WIND; MASS-LOSS; GRAINS; GAS
AB Aims. We model the synthesis of molecules and dust in the inner wind of the oxygen-rich Mira-type star IK Tau by considering the effects of periodic shocks induced by the stellar pulsation on the gas and by following the non-equilibrium chemistry in the shocked gas layers between 1 R-star and 10 R-star. We consider a very complete set of molecules and dust clusters, and combine the nucleation phase of dust formation with the condensation of these clusters into dust grains. We also test the impact of increasing the local gas density. Our derived molecular abundances and dust properties are compared to the most recent observational data.
Methods. A semi-analytical formalism based on parameterised fluid equations is used to describe the gas density, velocity, and temperature in the inner wind. The chemistry is described by using a chemical kinetic network of reactions and the condensation mechanism is described by a Brownian formalism. A set of stiff, ordinary, coupled differential equations is solved, and molecular abundances, dust cluster abundances, grain size distributions and dust masses are derived.
Results. The shocks drive an active non-equilibrium chemistry in the dust formation zone of IK Tau where the collision destruction of CO in the post-shock gas triggers the formation of C-bearing species such as HCN and CS. Most of the modelled molecular abundances agree well with the latest values derived from Herschel data, except for SO2 and NH3, whose formation may not occur in the inner wind. Clusters of alumina, Al2O3, are produced within 2 R-star and lead to a population of alumina grains close to the stellar surface. Clusters of silicates (Mg2SiO4) form at larger radii (r > 3 R-star), where their nucleation is triggered by the formation of HSiO and H2SiO. They efficiently condense and reach their final grain size distribution between similar to 6 R-star and 8 R-star with a major population of medium size grains peaking at similar to 200 angstrom. This two dust-shell configuration agrees with recent interferometric observations. The derived dust-to-gas mass ratio for IK Tau is in the range 1-6 x 10(-3) and agrees with values derived from observations of O-rich Mira-type stars.
Conclusions. Our results confirm the importance of periodic shocks in chemically shaping the inner wind of AGB stars and providing gas conditions conducive to the efficient synthesis of molecules and dust by non-equilibrium processes. They indicate that the wind acceleration will possibly develop in the radius range 4-8 R-star in IK Tau.
C1 [Gobrecht, D.] INAF, Osservatorio Astron Teramo, I-64100 Teramo, Italy.
[Gobrecht, D.; Cherchneff, I.] Univ Basel, Dept Phys, Klingelbergstr 82, CH-4056 Basel, Switzerland.
[Sarangi, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sarangi, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Plane, J. M. C.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Bromley, S. T.] Univ Barcelona, Dept Quim Fis, Mart i Franques 1, E-08028 Barcelona, Spain.
[Bromley, S. T.] ICREA, Barcelona 08010, Spain.
RP Cherchneff, I (reprint author), Univ Basel, Dept Phys, Klingelbergstr 82, CH-4056 Basel, Switzerland.
EM isabelle.cherchneff@unibas.ch
RI Bromley, Stefan/A-2481-2009; Plane, John/C-7444-2015
OI Bromley, Stefan/0000-0002-7037-0475; Plane, John/0000-0003-3648-6893
FU Swiss National Science Foundation [200021_132616, 200020_149190]
FX The authors thank the anonymous referee for comments that have improved
the quality of the manuscript and Nicolas Mauron for stimulating
discussions. D.G. acknowledges support from the Swiss National Science
Foundation grants 200021_132616 and 200020_149190.
NR 79
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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 JAN
PY 2016
VL 585
AR A6
DI 10.1051/0004-6361/201425363
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300013
ER
PT J
AU Kreikenbohm, A
Schulz, R
Kadler, M
Wilms, J
Markowitz, A
Chang, CS
Carpenter, B
Elsasser, D
Gehrels, N
Mannheim, K
Muller, C
Ojha, R
Ros, E
Trustedt, J
AF Kreikenbohm, A.
Schulz, R.
Kadler, M.
Wilms, J.
Markowitz, A.
Chang, C. S.
Carpenter, B.
Elsaesser, D.
Gehrels, N.
Mannheim, K.
Mueller, C.
Ojha, R.
Ros, E.
Truestedt, J.
TI The gamma-ray emitting radio-loud narrow-line Seyfert 1 galaxy PKS
2004-447 I. The X-ray View
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: individual: PKS 2004-447; galaxies: jets;
galaxies: Seyfert; quasars: general; X-rays: general
ID ACTIVE GALACTIC NUCLEI; COMPACT STEEP-SPECTRUM; LARGE-AREA TELESCOPE;
PHOTON IMAGING CAMERA; XMM-NEWTON; PMN J0948+0022; FERMI BLAZARS;
ENERGY-DISTRIBUTION; SUZAKU OBSERVATION; ASCA OBSERVATIONS
AB As part of the TANAMI multiwavelength progam, we discuss new X-ray observations of the gamma-ray and radio-loud narrow line Seyfert 1 galaxy (gamma-NLS1) PKS 2004 447. The active galaxy is a member of a small sample of radio-loud NLS1s detected in gamma-rays by the Fermi Large Area Telescope. It stands out for being the radio-loudest and the only southern-hemisphere source in this sample. We present results from our X-ray monitoring program comprised of Swift snapshot observations from 2012 through 2014 and two new X-ray observations with XMM-Newton in 2012. Supplemented by archival data from 2004 and 2011, our data set allows for a careful analysis of the X-ray spectrum and variability of this peculiar source. The (0.5-10) keV spectrum is described well by a power law (Gamma similar to 1.6), which can be interpreted as non-thermal emission from a relativistic jet. The source exhibits moderate flux variability on timescales of both months and years. Correlated brightness variations in the (0.5-2) keV and (2-10) keV bands are explained by a single variable spectral component, such as the one from the jet. A possible soft excess seen in the data from 2004 cannot be confirmed by the new XMM-Newton observations taken during low-flux states. Any contribution to the total flux in 2004 is less than 20% of the power-law component. The (0.5-10) keV luminosities of PKS 2004 447 are in the range of (0.5-2.7) x 10(44) erg s(-1). A comparison of the X-ray properties among the known gamma-NLS1 galaxies shows that in four out of five cases the X-ray spectrum is dominated by a flat power law without intrinsic absorption. These objects are moderately variable in their brightness, while spectral variability is observed in at least two sources. The major difference across the X-ray spectra of gamma-NLS1s is the luminosity, which spans a range of almost two orders of magnitude from 10(44) erg s(-1) to 10(46) erg s(-1) in the (0.5-10) keV band.
C1 [Kreikenbohm, A.; Schulz, R.; Kadler, M.; Elsaesser, D.; Mannheim, K.; Mueller, C.; Truestedt, J.] Univ Wurzburg, Lehrstuhl Astron, Campus Hubland Nord,Emil Fischer Str 31, D-97074 Wurzburg, Germany.
[Kreikenbohm, A.; Schulz, R.; Wilms, J.; Markowitz, A.] Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
[Kreikenbohm, A.; Schulz, R.; Wilms, J.; Markowitz, A.] Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany.
[Markowitz, A.] Univ Calif San Diego, CASS, 9500 Gilman Dr,MC 0424, La Jolla, CA 92093 USA.
[Chang, C. S.] Joint ALMA Observ, ESO, Santiago 7630355, Chile.
[Carpenter, B.; Gehrels, N.; Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Carpenter, B.; Mueller, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA.
[Ojha, R.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Ros, E.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Ros, E.] Univ Valencia, Observ Astron, Paterna Valencia 46980, Spain.
[Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
RP Kreikenbohm, A (reprint author), Univ Wurzburg, Lehrstuhl Astron, Campus Hubland Nord,Emil Fischer Str 31, D-97074 Wurzburg, Germany.; Kreikenbohm, A (reprint author), Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.; Kreikenbohm, A (reprint author), Erlangen Ctr Astroparticle Phys, Sternwartstr 7, D-96049 Bamberg, Germany.
EM akreikenbohm@astro.uni-wuerzburg.de
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Ros, Eduardo/0000-0001-9503-4892;
Kadler, Matthias/0000-0001-5606-6154
FU Bundesministerium fur Wirtschaft und Technologie through the Deutsches
Zentrum fur Luft- und Raumfahrt [50 OR 1303]; Deutsche
Forschungsgemeinschaft [WI 1860/10-1]; Spanish MINECO
[AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat Valenciana
project [PROMETEO/2009/104, PROMETEOII/2014/057]; MP0905 action "Black
Holes in a Violent Universe"; EU Framework 6 Marie Curie Early Stage
Training program [MEST-CT-2005-19669]; NASA through Fermi Guest
Investigator grants [NNH10ZDA001N, NNH12ZDA001N, 41213, 61089]; ESA
Member States; USA (NASA); Swift, a NASA mission
FX We acknowledge support by the Bundesministerium fur Wirtschaft und
Technologie through the Deutsches Zentrum fur Luft- und Raumfahrt
contract 50 OR 1303, the Deutsche Forschungsgemeinschaft under contract
WI 1860/10-1, the Spanish MINECO projects AYA2009-13036-C02-02,
AYA2012-38491-C02-01, and by the Generalitat Valenciana project
PROMETEO/2009/104 and PROMETEOII/2014/057. E.R. and C.S.C. were
partially supported by the MP0905 action "Black Holes in a Violent
Universe". C.S.C. was supported by the EU Framework 6 Marie Curie Early
Stage Training program under contract number MEST-CT-2005-19669
"ESTRELA". This research made use of a collection of ISIS scripts
provided by the Dr. Karl Remeis observatory, Bamberg, Germany at
http://www.sternwarte.uni-erlangen.de/isis/. This research was funded in
part by NASA through Fermi Guest Investigator grants NNH10ZDA001N and
NNH12ZDA001N (proposal numbers 41213 and 61089). This research was
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. This research makes use of
data obtained by XMM-Newton, an ESA science mission funded by ESA Member
States and the USA (NASA), and Swift, a NASA mission with international
participation.
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2016
VL 585
AR A91
DI 10.1051/0004-6361/201424818
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300098
ER
PT J
AU Lorenzi, V
Pinilla-Alonso, N
Licandro, J
Cruikshank, DP
Grundy, WM
Binzel, RP
Emery, JP
AF Lorenzi, V.
Pinilla-Alonso, N.
Licandro, J.
Cruikshank, D. P.
Grundy, W. M.
Binzel, R. P.
Emery, J. P.
TI The spectrum of Pluto, 0.40-0.93 mu m I. Secular and longitudinal
distribution of ices and complex organics
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Kuiper belt objects: individual: Pluto; methods: observational; methods:
numerical; techniques: spectroscopic
ID SOLAR-SYSTEM BODIES; NEAR-INFRARED SPECTROSCOPY; CO-CONTAINING ICES;
OPTICAL-CONSTANTS; SURFACE; METHANE; TRITON; CHARON; N-2;
SPECTROPHOTOMETRY
AB Context. During the past 30 years the surface of Pluto has been characterized and its variability monitored through continuous nearinfrared spectroscopic observations. But in the visible range only a few data are available.
Aims. The aim of this work is to define Pluto's relative reflectance in the visible range to characterize the different components of its surface, and to provide ground based observations in support of the New Horizons mission.
Methods. We observed Pluto on six nights between May and July 2014 with the imager/spectrograph ACAM at the William Herschel Telescope (La Palma, Spain). The six spectra obtained cover a whole rotation of Pluto (P-rot = 6.4 days). For all the spectra, we computed the spectral slope and the depth of the absorption bands of methane ice between 0.62 and 0.90 mu m. To search for shifts in the center of the methane bands, which are associated with dilution of CH4 in N-2, we compared the bands with reflectances of pure methane ice.
Results. All the new spectra show the methane ice absorption bands between 0.62 and 0.90 mu m. Computation of the depth of the band at 0.62 mu m in the new spectra of Pluto and in the spectra of Makemake and Eris from the literature, allowed us to estimate the Lambert coefficient at this wavelength at temperatures of 30 K and 40 K, which has never been measured before. All the detected bands are blueshifted with respect to the position for pure methane ice, with minimum shifts correlated to the regions where the abundance of methane is higher. This could be indicative of a dilution of CH4:N-2 that is more saturated in CH4. The longitudinal and secular variations in the parameters measured in the spectra are in accordance with results previously reported in the literature and with the distribution of the dark and bright materials that show the Pluto's color maps from New Horizons.
C1 [Lorenzi, V.] Fdn Galileo Galilei INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain.
[Pinilla-Alonso, N.; Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, 1412 Circle Dr, Knoxville, TN 37996 USA.
[Licandro, J.] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, TF, Spain.
[Licandro, J.] Univ la Laguna, Dept Astrofis, Ave Astrofis Francisco Sanchez S-N, San Cristobal de la Laguna 38200, TF, Spain.
[Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Grundy, W. M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Binzel, R. P.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Lorenzi, V (reprint author), Fdn Galileo Galilei INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain.
EM lorenzi@tng.iac.es
FU Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias [055-WHT11/14A]; NASA's New Horizons mission;
MINECO, Spanish Ministry of Economy and Competitiveness
[ESP2013-47816-C4-2-P]
FX This paper is based on data from override observations made with the
William Herschel Telescope, under program 055-WHT11/14A, operated on the
island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
D.P.C., W.M.G., and R.P.B. were supported in part by NASA's New Horizons
mission. J.L. acknowledges support from the project ESP2013-47816-C4-2-P
(MINECO, Spanish Ministry of Economy and Competitiveness). We want to
thank the referee E. Lellouch for his valuable comments that improved
the manuscript.
NR 49
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2016
VL 585
AR A131
DI 10.1051/0004-6361/201527281
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300138
ER
PT J
AU Pajola, M
Lucchetti, A
Bertini, I
Marzari, F
A'Hearn, MF
La Forgia, F
Lazzarin, M
Naletto, G
Barbieri, C
AF Pajola, Maurizio
Lucchetti, Alice
Bertini, Ivano
Marzari, Francesco
A'Hearn, Michael F.
La Forgia, Fiorangela
Lazzarin, Monica
Naletto, Giampiero
Barbieri, Cesare
TI Size-frequency distribution of boulders >= 10 m on comet 103P/Hartley 2
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 103P/Hartley 2; methods: data
analysis
ID DEEP IMPACT; INSTRUMENT; NUCLEUS; IMAGES
AB Aims. We derive the size-frequency distribution of boulders on comet 103P/Hartley 2, which are computed from the images taken by the Deep Impact/HRI-V imaging system. We indicate the possible physical processes that lead to these boulder size distributions.
Methods. We used images acquired by the High Resolution Imager-Visible CCD camera on 4 November 2010. Boulders >= 10 m were identified and manually extracted from the datasets with the software ArcGIS. We derived the global size-frequency distribution of the illuminated side of the comet (similar to 50%) and identified the power-law indexes characterizing the two lobes of 103P. The three-pixel sampling detection, together with the shadowing of the surface, enables unequivocally detection of boulders scattered all over the illuminated surface.
Results. We identify 332 boulders >= 10 m on the imaged surface of the comet, with a global number density of nearly 140/km(2) and a cumulative size-frequency distribution represented by a power law with index of -2.7 +/- 0.2. The two lobes of 103P show similar indexes, i.e., -2.7 +/- 0.2 for the bigger lobe (called L1) and -2.6 + 0.2/-0.5 for the smaller lobe (called L2). The similar power-law indexes and similar maximum boulder sizes derived for the two lobes both point toward a similar fracturing/disintegration phenomena of the boulders as well as similar lifting processes that may occur in L1 and L2. The difference in the number of boulders per km(2) between L1 and L2 suggests that the more diffuse H2O sublimation on L1 produce twice the boulders per km(2) with respect to those produced on L2 (primary activity CO2 driven). The 103P comet has a lower global power-law index (-2.7 vs. -3.6) with respect to 67P. The global differences between the two comets' activities, coupled with a completely different surface geomorphology, make 103P hardly comparable to 67P. A shape distribution analysis of boulders >= 30 m performed on 103P suggests that the cometary boulders show more elongated shapes when compared to collisional laboratory fragments as well as to the boulders present on the surfaces of 25 143 Itokawa and 433 Eros asteroids. Consequently, this supports the interpretation that cometary boulders have different origins with respect to the impact-related asteroidal boulders.
C1 [Pajola, Maurizio; Lucchetti, Alice; Bertini, Ivano; Barbieri, Cesare] Univ Padua, Ctr Studies & Act Space, CISAS, G Colombo, Via Venezia 15, I-35131 Padua, Italy.
[Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lucchetti, Alice] INAF Astron Observ Padova, Vicolo Osservatorio 5, I-35131 Padua, Italy.
[Marzari, Francesco; La Forgia, Fiorangela; Lazzarin, Monica; Barbieri, Cesare] Univ Padua, Dept Phys & Astron G Galilei, Vic Osservatorio 3, I-35122 Padua, Italy.
[A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Naletto, Giampiero] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
[Naletto, Giampiero] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
RP Pajola, M (reprint author), Univ Padua, Ctr Studies & Act Space, CISAS, G Colombo, Via Venezia 15, I-35131 Padua, Italy.
EM maurizio.pajola@gmail.com
RI Naletto, Giampiero/S-6329-2016
OI Naletto, Giampiero/0000-0003-2007-3138
NR 23
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2016
VL 585
AR A85
DI 10.1051/0004-6361/201526834
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300092
ER
PT J
AU Puccetti, S
Comastri, A
Bauer, FE
Brandt, WN
Fiore, E
Harrison, FA
Luo, B
Stern, D
Urry, CM
Alexander, DM
Annuar, A
Arevalo, P
Balokovic, M
Boggs, SL
Brightman, M
Christensen, FE
Craig, WW
Gandhi, P
Hailey, CJ
Koss, MJ
La Massa, S
Marinucci, A
Ricci, C
Walton, DJ
Zappacosta, L
Zhang, W
AF Puccetti, S.
Comastri, A.
Bauer, F. E.
Brandt, W. N.
Fiore, E.
Harrison, F. A.
Luo, B.
Stern, D.
Urry, C. M.
Alexander, D. M.
Annuar, A.
Arevalo, P.
Balokovic, M.
Boggs, S. L.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Hailey, C. J.
Koss, M. J.
La Massa, S.
Marinucci, A.
Ricci, C.
Walton, D. J.
Zappacosta, L.
Zhang, W.
TI Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed
by NuSTAR
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: individual: NGC 6240; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEUS; STAR-FORMATION RATE; BLACK-HOLE GROWTH;
XMM-NEWTON; STARBURST GALAXIES; INTERACTING GALAXY; EDDINGTON RATIO;
QUASAR FEEDBACK; LINE EMISSION; HOST GALAXIES
AB We present a broadband (similar to 0.3-70 keV) spectral and temporal analysis of NuSTAR observations of the luminous infrared galaxy NGC 6240 combined with archival Chandra, XMM-Newton, and BeppoSAX data. NGC 6240 is a galaxy in a relatively early merger state with two distinct nuclei separated by similar to 1.''5. Previous Chandra observations resolved the two nuclei and showed that they are both active and obscured by Compton-thick material. Although they cannot be resolved by NuSTAR, we were able to clearly detect, for the first time, both the primary and the reflection continuum components thanks to the unprecedented quality of the NuSTAR data at energies >10 keV. The NuSTAR hard X-ray spectrum is dominated by the primary continuum piercing through an absorbing column density which is mildly optically thick to Compton scattering (tau similar or equal to 1.2, N-H similar to 1.5 x 10(24) cm(-2)). We detect moderately hard X-ray (>10 keV) flux variability up to 20% on short (15-20 ks) timescales. The amplitude of the variability is largest at similar to 30 keV and is likely to originate from the primary continuum of the southern nucleus. Nevertheless, the mean hard X-ray flux on longer timescales (years) is relatively constant. Moreover, the two nuclei remain Compton-thick, although we find evidence of variability in the material along the line of sight with column densities N-H <= 2 x 1023 cm(-2) over long (similar to 3-15 yr) timescales. The observed X-ray emission in the NuSTAR energy range is fully consistent with the sum of the best-fit models of the spatially resolved Chandra spectra of the two nuclei.
C1 [Puccetti, S.] ASDC ASI, Via Politecn, I-00133 Rome, Italy.
[Puccetti, S.; Fiore, E.; Zappacosta, L.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy.
[Comastri, A.] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Bauer, F. E.; Arevalo, P.; Ricci, C.] EMBIGGEN Anillo, Concepcion, Chile.
[Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 6177, Santiago 22, Chile.
[Bauer, F. E.] Millenium Inst Astrophys, Casilla 360, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA.
[Harrison, F. A.; Balokovic, M.; Brightman, M.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA.
[Urry, C. M.; La Massa, S.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA.
[Alexander, D. M.; Annuar, A.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
[Boggs, S. L.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] 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.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M. J.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
[Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Puccetti, S (reprint author), ASDC ASI, Via Politecn, I-00133 Rome, Italy.
EM puccetti@asdc.asi.it
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Urry, Meg/0000-0002-0745-9792
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
ASI/INAF [I/037/12/0 - 011/13]; Caltech NuSTAR [44A-1092750];
CONICYT-Chile [Basal-CATA PFB-06/2007, FONDECYT 1141218]; "EMBIGGEN"
Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's
Millennium Science Initiative [IC120009]; NASA Headquarters under the
NASA Earth and Space Science Fellowship Program [NNX14AQ07H]
FX This work was supported under NASA Contract 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). A.C., A.M., F.F. and L.Z. acknowledge support from
the ASI/INAF grant I/037/12/0 - 011/13. W.N.B. acknowledges support from
Caltech NuSTAR sub-contract 44A-1092750. F.E.B. and C.R. acknowledge
support from CONICYT-Chile grants Basal-CATA PFB-06/2007 and FONDECYT
1141218. F.E.B., C.R. and P.A. acknowledge support from "EMBIGGEN"
Anillo ACT1101. FEB acknowledges support from the Ministry of Economy,
Development, and Tourism's Millennium Science Initiative through grant
IC120009, awarded to The Millennium Institute of Astrophysics, MAS. M.B.
acknowledges support from NASA Headquarters under the NASA Earth and
Space Science Fellowship Program, grant NNX14AQ07H.
NR 92
TC 5
Z9 5
U1 2
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 JAN
PY 2016
VL 585
AR A157
DI 10.1051/0004-6361/201527189
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300164
ER
PT J
AU Titarchuk, L
Seifina, E
AF Titarchuk, Lev
Seifina, Elena
TI Scaling of the photon index vs. mass accretion rate correlation and
estimate of black hole mass in M101 ULX-1
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; radiation mechanisms: general; black hole
physics
ID X-RAY SOURCES; HUBBLE-SPACE-TELESCOPE; MONTE-CARLO SIMULATIONS;
VARIABILITY CHARACTERISTICS; SPECTRAL INDEX; XTE J1550-564;
NEUTRON-STAR; KEY PROJECT; OUTBURST; BINARIES
AB We report the results of Swift and Chandra observations of an ultraluminous X-ray source, ULX-1 in M101. We show strong observational evidence that M101 ULX-1 undergoes spectral transitions from the low/hard state to the high/soft state during these observations. The spectra of M101 ULX-1 are well fitted by the so-called bulk motion Comptonization (BMC) model for all spectral states. We have established the photon index (Gamma) saturation level, Gamma(sat) = 2.8 +/- 0.1, in the Gamma versus mass accretion rate ((M) over dot) correlation. This Gamma - (M) over dot correlation allows us to evaluate black hole (BH) mass in M101 ULX-1 to be M-BH similar to (3.2-4.3) x 10(4) M-circle dot, assuming the spread in distance to M101 (from 6.4 +/- 0.5 Mpc to 7.4 +/- 0.6 Mpc). For this BH mass estimate we apply the scaling method, using Galactic BHs XTE J1550-564, H 1743-322 and 4U 1630-472 as reference sources. The Gamma vs. (M) over dot correlation revealed in M101 ULX-1 is similar to that in a number of Galactic BHs and clearly exhibits the correlation along with the strong Gamma saturation at approximate to 2.8. This is robust observational evidence for the presence of a BH in M101 ULX-1. We also find that the seed (disk) photon temperatures are low, on the order of 40-100 eV, which is consistent with high BH mass in M101 ULX-1. Thus, we suggest that the central object in M101 ULX-1 has intermediate BH mass on the order of 10(4) solar masses.
C1 [Titarchuk, Lev] Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44122 Ferrara, Italy.
[Titarchuk, Lev] Natl Res Nucl Univ MEPhI Moscow Engn Phys Inst, Moscow 115409, Russia.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20770 USA.
[Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia.
RP Titarchuk, L (reprint author), Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44122 Ferrara, Italy.; Titarchuk, L (reprint author), Natl Res Nucl Univ MEPhI Moscow Engn Phys Inst, Moscow 115409, Russia.; Titarchuk, L (reprint author), NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20770 USA.; Seifina, E (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia.
EM titarchuk@fe.infn.it; seif@sai.msu.ru
NR 49
TC 2
Z9 2
U1 0
U2 0
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 JAN
PY 2016
VL 585
AR A94
DI 10.1051/0004-6361/201526122
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD1VI
UT WOS:000369710300101
ER
PT J
AU Kishore, P
Jyothi, S
Basha, G
Rao, SVB
Rajeevan, M
Velicogna, I
Sutterley, TC
AF Kishore, P.
Jyothi, S.
Basha, Ghouse
Rao, S. V. B.
Rajeevan, M.
Velicogna, Isabella
Sutterley, Tyler C.
TI Precipitation climatology over India: validation with observations and
reanalysis datasets and spatial trends
SO CLIMATE DYNAMICS
LA English
DT Article
DE Precipitation; Climatology; India; IMD; GPCC; APHRODITE; ERA-Interim;
CFSR; JRA-25; MERRA; Trends; Validation
ID ASIAN SUMMER MONSOON; RAINFALL; PERFORMANCE; JRA-25
AB Changing rainfall patterns have significant effect on water resources, agriculture output in many countries, especially the country like India where the economy depends on rain-fed agriculture. Rainfall over India has large spatial as well as temporal variability. To understand the variability in rainfall, spatial-temporal analyses of rainfall have been studied by using 107 (1901-2007) years of daily gridded India Meteorological Department (IMD) rainfall datasets. Further, the validation of IMD precipitation data is carried out with different observational and different reanalysis datasets during the period from 1989 to 2007. The Global Precipitation Climatology Project data shows similar features as that of IMD with high degree of comparison, whereas Asian Precipitation-Highly-Resolved Observational Data Integration Towards Evaluation data show similar features but with large differences, especially over northwest, west coast and western Himalayas. Spatially, large deviation is observed in the interior peninsula during the monsoon season with National Aeronautics Space Administration-Modern Era Retrospective-analysis for Research and Applications (NASA-MERRA), pre-monsoon with Japanese 25 years Re Analysis (JRA-25), and post-monsoon with climate forecast system reanalysis (CFSR) reanalysis datasets. Among the reanalysis datasets, European Centre for Medium-Range Weather Forecasts Interim Re-Analysis (ERA-Interim) shows good comparison followed by CFSR, NASA-MERRA, and JRA-25. Further, for the first time, with high resolution and long-term IMD data, the spatial distribution of trends is estimated using robust regression analysis technique on the annual and seasonal rainfall data with respect to different regions of India. Significant positive and negative trends are noticed in the whole time series of data during the monsoon season. The northeast and west coast of the Indian region shows significant positive trends and negative trends over western Himalayas and north central Indian region.
C1 [Kishore, P.; Velicogna, Isabella; Sutterley, Tyler C.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Jyothi, S.; Rao, S. V. B.] Sri Venkateswara Univ, Dept Phys, Tirupati 517502, Andhra Pradesh, India.
[Basha, Ghouse] Masdar Inst Sci & Technol, Inst Ctr Water & Environm iWATER, POB 54224, Abu Dhabi, U Arab Emirates.
[Rajeevan, M.] Minist Earth Sci, Prithvi Bhavan,Mausam Bhavan Campus, New Delhi, India.
[Velicogna, Isabella] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kishore, P (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM kishore1818@gmail.com
RI Sutterley, Tyler/Q-8325-2016;
OI Sutterley, Tyler/0000-0002-6964-1194; Vijaya Bhaskara Rao,
Sarangam/0000-0002-8755-027X; RAJEEVAN, Madhavan/0000-0002-3000-2459
FU UGC, New Delhi
FX We would like to thank all the members of CFSR, ERA-Interim, JRA-25, and
NASA-MERRA reanalysis data centers for the public access of their data
via their webpages. Authors are thankful to APHRODITE and GPCP
observational data centers. The authors are thankful to the India
Meteorological Department (IMD) for providing the rainfall gridded
datasets. The second author (SJ) acknowledges to UGC, New Delhi for
providing the fellowship UGS-SVU Centre for MST Radar Applications
during my course of work.
NR 44
TC 6
Z9 6
U1 4
U2 8
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2016
VL 46
IS 1-2
BP 541
EP 556
DI 10.1007/s00382-015-2597-y
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD6NE
UT WOS:000370040100034
ER
PT J
AU Jousse, A
Hall, A
Sun, F
Teixeira, J
AF Jousse, A.
Hall, A.
Sun, F.
Teixeira, J.
TI Causes of WRF surface energy fluxes biases in a stratocumulus region
SO CLIMATE DYNAMICS
LA English
DT Article
DE Stratocumulus; Surface energy fluxes; Weather Research and Forecasting
(WRF) model; Physics parameterization schemes; VOCALS-REx
ID BOUNDARY-LAYER CLOUDS; SOUTHEAST PACIFIC; BULK PARAMETERIZATION;
CLOSURE-MODEL; VOCALS-REX; PART II; CONVECTION; TURBULENCE;
PRECIPITATION; CUMULUS
AB In this study, we evaluate the ability of the Weather Research and Forecasting model to simulate surface energy fluxes in the southeast Pacific stratocumulus region. A total of 18 simulations is performed for the period of October to November 2008, with various combinations of boundary layer, microphysics, and cumulus schemes. Simulated surface energy fluxes are compared to those measured during VOCALS-REx. Using a process-based model evaluation, errors in surface fluxes are attributed to errors in cloud properties. Net surface flux errors are mostly traceable to errors in cloud liquid water path (LWPcld), which produce biases in downward shortwave radiation. Two mechanisms controlling LWPcld are diagnosed. One involves microphysics schemes, which control LWPcld through the production of raindrops. The second mechanism involves boundary layer and cumulus schemes, which control moisture available for cloud by regulating boundary layer height. In this study, we demonstrate that when parameterizations are appropriately chosen, the stratocumulus deck and the related surface energy fluxes are reasonably well represented. In the most realistic experiments, the net surface flux is underestimated by about 10 W m(-2). This remaining low bias is due to a systematic overestimation of the total surface cooling due to sensible and latent heat fluxes in our simulations. There does not appear to be a single physical reason for this bias. Finally, our results also suggest that inaccurate representation of boundary layer height is an important factor limiting further gains in model realism.
C1 [Jousse, A.; Hall, A.; Sun, F.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Teixeira, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Jousse, A (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
EM jousse@atmos.ucla.edu
FU Department of Energy (DOE) [DE-SC0001467]; National Science Foundation
(NSF) [EF-106585]
FX This work was supported by the Department of Energy (DOE) Grant
#DE-SC0001467 and the National Science Foundation (NSF) Grant
#EF-106585. MODIS data were downloaded from the NASA Web site (available
at http://ladsweb.nascom.nasa.gov). VOCALS-REx data were downloaded from
the National Center for Atmospheric Research (NCAR) Environmental
Observing Laboratory (EOL) data archive (available at
http://www.eol.ucar.edu/projects/vocals/). We thank Drs. Florent Brient,
Hsin-Yuan Huang and Xin Qu for many stimulating discussions on the
topic.
NR 41
TC 2
Z9 2
U1 2
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2016
VL 46
IS 1-2
BP 571
EP 584
DI 10.1007/s00382-015-2599-9
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD6NE
UT WOS:000370040100036
ER
PT J
AU Su, Z
Xi, X
Natraj, V
Li, KF
Shia, RL
Miller, CE
Yung, YL
AF Su, Zhan
Xi, Xi
Natraj, Vijay
Li, King-Fai
Shia, Run-Lie
Miller, Charles E.
Yung, Yuk L.
TI Information-rich spectral channels for simulated retrievals of partial
column-averaged methane
SO EARTH AND SPACE SCIENCE
LA English
DT Article
DE remote sensing; information analysis; channel selection; methane cycle
ID GASES OBSERVING SATELLITE; ATMOSPHERIC METHANE; REFLECTED SUNLIGHT; MOLE
FRACTIONS; CH4; CO2; RESOLUTION; ALGORITHM; NETWORK; AEROSOL
AB Space-based remote sensing of the column-averaged methane dry air mole fraction (XCH4) has greatly increased our understanding of the spatiotemporal patterns in the global methane cycle. The potential to retrieve multiple pieces of vertical profile information would further improve the quantification of CH4 across space-time scales. We conduct information analysis for channel selection and evaluate the prospects of retrieving multiple pieces of information as well as total column CH4 from both ground-based and space-based near-infrared remote sensing spectra. We analyze the degrees of freedom of signal (DOF) in the CH4 absorption bands near 2.3m and 1.6m and select approximate to 1% of the channels that contain >95% of the information about the CH4 profile. The DOF is around 4 for fine ground-based spectra (resolution=0.01cm(-1)) and 3 for coarse space-based spectra (resolution=0.20cm(-1)) based on channel selection and a signal-to-noise ratio (SNR) of 300. The DOF varies from 2.2 to 3.2 when SNR is between 100 and 300, and spectral resolution is 0.20cm(-1). Simulated retrieval tests in clear-sky conditions using the selected channels reveal that the retrieved partial column-averaged CH4 values are not sensitive to the a priori profiles and can reflect local enhancements of CH4 in different partial air columns. Both the total and partial column-averaged retrieval errors in all tests are within 1% of the true state. These simulated tests highlight the possibility to retrieve up to three to four pieces of information about the vertical distribution of CH4 in reality.
C1 [Su, Zhan; Xi, Xi; Li, King-Fai; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Natraj, Vijay; Miller, Charles E.; Yung, Yuk L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Li, King-Fai] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA.
RP Xi, X (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM zssu@caltech.edu
OI Li, King-Fai/0000-0003-0150-2910
NR 59
TC 1
Z9 1
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 EARTH SPACE SCI
JI Earth Space Sci.
PD JAN
PY 2016
VL 3
IS 1
BP 2
EP 14
DI 10.1002/2015EA000120
PG 13
WC Geosciences, Multidisciplinary
SC Geology
GA DE6NS
UT WOS:000370751400001
ER
PT J
AU Huang, HT
Kim, SB
Tsang, L
Xu, XL
Liao, TH
Jackson, TJ
Yueh, SH
AF Huang, Huanting
Kim, Seung-Bum
Tsang, Leung
Xu, Xiaolan
Liao, Tien-Hao
Jackson, Thomas J.
Yueh, Simon H.
TI Coherent Model of L-Band Radar Scattering by Soybean Plants: Model
Development, Evaluation, and Retrieval
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Analytical method; coherent model; data-cube; mutual exclusion; soil
moisture retrieval; soybean
ID SOIL-MOISTURE RETRIEVAL; ELECTROMAGNETIC SCATTERING; VEGETATION;
BACKSCATTERING; CANOPY; INVERSION; SURFACES; LAYER
AB An improved coherent branching model for L-band radar remote sensing of soybean is proposed by taking into account the correlated scattering among scatterers. The novel feature of the analytical coherent model consists of conditional probability functions to eliminate the overlapping effects of branches in the former branching models. Backscattering coefficients are considered for a variety of scenarios over the full growth cycle for vegetation water content (VWC) and the complete drydown conditions for soil moisture. The results of the coherent model show that HH scattering has a significant difference up to 3 dB from that of the independent scattering when VWC is low, e.g., 0.2 kg/m(2). Forward model calculations are performed for the scattering from the soybean field for the full range of three axes of root-mean-square (RMS) height of bare soil, VWC, and soil moisture using the coherent model. The soybean volume scattering including the double-bounce term is combined with the back scattering of bare soil from the numerical Maxwell solutions that incorporates RMS height, soil permittivity, and correlation length, to form the forward model lookup table for the vegetated soil. The results are compared with data from 13 soybean fields collected as part of the soil moisture active passive validation experiment 2012 (SMAPVEX12). Time-series retrieval of soil moisture is also applied to the soybean fields by inverting the forward model lookup table. During the retrieval, the VWC is optimized with physical constraints obtained from ground measurements. The retrieval performances are significantly improved using the proposed coherent model: the root-mean-squared error (RMSE) of the soil moisture retrieval is decreased from 0.09 to 0.05 cm(3)/cm(3) and the correlation coefficient is increased from 0.66 to 0.92.
C1 [Huang, Huanting; Tsang, Leung; Liao, Tien-Hao] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA.
[Huang, Huanting; Tsang, Leung; Liao, Tien-Hao] Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48103 USA.
[Kim, Seung-Bum; Xu, Xiaolan; Yueh, Simon H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Jackson, Thomas J.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
RP Huang, HT (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA.; Huang, HT (reprint author), Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48103 USA.
FU NASA SMAP project
FX The authors would like to thank NASA SMAP project to support the work
and the measurement data provided by the SMAPVEX12 field campaign. The
U.S. Department of Agriculture is an Equal Opportunity Employer. They
would also like to thank the reviewers for numerous comments that helped
significantly improve the paper.
NR 26
TC 1
Z9 1
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD JAN
PY 2016
VL 9
IS 1
BP 272
EP 284
DI 10.1109/JSTARS.2015.2469717
PG 13
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3PE
UT WOS:000370541400029
ER
PT J
AU Sadeghi, Y
St-Onge, B
Leblon, B
Simard, M
AF Sadeghi, Yaser
St-Onge, Benoit
Leblon, Brigitte
Simard, Marc
TI Canopy Height Model (CHM) Derived From a TanDEM-X InSAR DSM and an
Airborne Lidar DTM in Boreal Forest
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Canopy surface height (CSH); dominant height (DH); lidar CHM; TanDEM-X
canopy height model (CHM)
ID 3D VEGETATION STRUCTURE; SCATTERING PHASE CENTER; ABOVEGROUND BIOMASS;
SAR INTERFEROMETRY; POL-INSAR; POLARIMETRIC RADAR; L-BAND; MISSION;
CARBON; SRTM
AB The first global X-band spaceborne single-pass interferometer mission, TanDEM-X, provides a spatially continuous map of global canopy elevations. In this paper, we assess the use of TanDEM-X data, in combination with an external digital terrain model (DTM), tomap boreal canopy heights. A comparison of the TanDEM-X canopy height model (CHM) to a validated reference lidar CHMwas performed based on two definitions of canopy height: canopy surface height (CSH) and dominant height (DH) at spatial resolutions ranging from 5 to 25 m, and at stand level. We found the TanDEM-X CHM to have a coarser resolution than the corresponding lidar CHM. This was apparent in the height validation of the TanDEM-X CHM, which had a RMSE of 2.7 m at the 5-m resolution, 1.9 mat the 25-m resolution, and 1.5m at stand level. The height differences between the InSAR and lidar surfaces varied between 1.3 and 1.5 m, but InSAR heights were below the height of dominant trees by 4.6-7.5 m. Similar discrepancies were observed for the lidar CSH relatively to DH (6.04, 8.98, and 8.05 m, respectively). The results show that the TanDEM-X interferometric heights are very close to the lidar reference height and that penetration below the DH is caused by propagation of the microwave signal between the tree apices and the main foliage surface in boreal forest. Finally, the accuracy of InSAR height estimates was not sensitive to tree density effects, but was moderately affected by local incidence angles (LIAs), gap volume, and canopy height.
C1 [Sadeghi, Yaser] Univ Quebec Montreal UQAM, Dept Sci, Inst Environm Sci, Montreal, PQ H2S 2Y4, Canada.
[St-Onge, Benoit] Univ Quebec Montreal UQAM, Dept Geog, Montreal, PQ H3C 3P8, Canada.
[Leblon, Brigitte] Univ New Brunswick, Fac Forestry & Environm Management, Fredericton, NB E3B 5A3, Canada.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Sadeghi, Y (reprint author), Univ Quebec Montreal UQAM, Dept Sci, Inst Environm Sci, Montreal, PQ H2S 2Y4, Canada.; St-Onge, B (reprint author), Univ Quebec Montreal UQAM, Dept Geog, Montreal, PQ H3C 3P8, Canada.; Leblon, B (reprint author), Univ New Brunswick, Fac Forestry & Environm Management, Fredericton, NB E3B 5A3, Canada.; Simard, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM st-onge.benoit@uqam.ca; bleblon@unb.ca; marc.simard@jpl.nasa.gov
RI Simard, Marc/H-3516-2013
OI Simard, Marc/0000-0002-9442-4562
FU Natural Sciences and Engineering Council of Canada; NASA's USPI
FX This work was supported by the Natural Sciences and Engineering Council
of Canada. The work of M. Simard was supported by NASA's USPI (US
Participating Investigator) program.
NR 74
TC 1
Z9 2
U1 6
U2 16
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD JAN
PY 2016
VL 9
IS 1
BP 381
EP 397
DI 10.1109/JSTARS.2015.2512230
PG 17
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3PE
UT WOS:000370541400039
ER
PT J
AU Egan, K
Alonso, AL
Jose, B
Gilmartin, N
McCluskey, P
Byrne, B
Ricco, A
Kenny, D
AF Egan, K.
Alonso, Lopez A.
Jose, B.
Gilmartin, N.
McCluskey, P.
Byrne, B.
Ricco, A.
Kenny, D.
TI A Novel Platelet Function Test Rapidly Detects Drug Effects in Patients
with Cardiovascular Disease
SO IRISH JOURNAL OF MEDICAL SCIENCE
LA English
DT Meeting Abstract
C1 [Egan, K.; Alonso, Lopez A.; Kenny, D.] Royal Coll Surgeons Ireland, Dublin 2, Ireland.
[Egan, K.; Alonso, Lopez A.; Jose, B.; Gilmartin, N.; McCluskey, P.; Byrne, B.; Ricco, A.; Kenny, D.] Dublin City Univ, Biomed Diagnost Inst, Dublin 9, Ireland.
[Ricco, A.] NASA, Ames Res Ctr, Moffett Field, CA USA.
RI Kenny, Dermot/C-3898-2012
NR 0
TC 0
Z9 0
U1 1
U2 2
PU SPRINGER LONDON LTD
PI LONDON
PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND
SN 0021-1265
EI 1863-4362
J9 IRISH J MED SCI
JI Irish J. Med. Sci.
PD JAN
PY 2016
VL 185
SU 1
BP S37
EP S38
PG 2
WC Medicine, General & Internal
SC General & Internal Medicine
GA DE1IN
UT WOS:000370380600076
ER
PT J
AU Goornavar, V
Biradar, S
Periyakaruppan, A
Koehne, J
Ramesh, GT
AF Goornavar, Virupaxi
Biradar, Santoshkumar
Periyakaruppan, Adaikkappan
Koehne, Jessica
Ramesh, Govindarajan T.
TI Optimization of Parameters to Achieve High Yield and Purity
Single-Walled Carbon Nanotube by Thermal and Chemical Oxidation and Its
Effect on Conductivity
SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY
LA English
DT Article
DE Single Wall Carbon Nanotube; FESEM; TEM; TGA; Conductivity
ID PURIFICATION; METAL; DECOMPOSITION; ELECTRODES; REMOVAL; GROWTH; CO
AB Single wall carbon nanotubes due to their unique structural and electronic characteristics have revolutionized the field of nanotechnology and are widely used the field of transistors, drug delivery, and nanocomposities. For improved efficiency of these applications, the utilized tubes must of preeminent purity. Here, we report key parameters that are optimized to achieve their highest purity upto 98 wt%, and yield as high as 50 wt% by thermal and chemical oxidation. The as -produced SWCNT were heated in air at 470 C, for 90 min, and later subjected to chemical oxidation. The chemical oxidation involved the treatment of thermally treated SWCNT with different concentrations of HCI (4N, 6N, 8N) and 30% H2O2, for different time periods (4 hr, 6 hr). This method does not cause damage to the walls of the tubes, observing no loss of nanotubes. The sheet resistance of as -produced and purified tubes was measured and the conductivity was calculated.
C1 [Goornavar, Virupaxi; Ramesh, Govindarajan T.] Norfolk State Univ, Mol Toxicol Lab, Ctr Biotechnol & Biomed Sci, 700 Pk Ave, Norfolk, VA 23504 USA.
[Goornavar, Virupaxi; Ramesh, Govindarajan T.] Norfolk State Univ, Ctr Mat Res, 555 Pk Ave, Norfolk, VA 23504 USA.
[Biradar, Santoshkumar] Rice Univ, Houston, TX 77251 USA.
[Koehne, Jessica] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ramesh, GT (reprint author), Norfolk State Univ, Mol Toxicol Lab, Ctr Biotechnol & Biomed Sci, 700 Pk Ave, Norfolk, VA 23504 USA.; Ramesh, GT (reprint author), Norfolk State Univ, Ctr Mat Res, 555 Pk Ave, Norfolk, VA 23504 USA.
FU NSF-CREST (CNBMD)-HRD [1036494]; DOD [(CEAND)-W911NF-11-1-0209]; NASA
NSTI
FX This work was supported by NSF-CREST (CNBMD)-HRD 1036494, DOD
(CEAND)-W911NF-11-1-0209 (US Army Research Office) and NASA NSTI. We
thank Dr. S. S. Sun, Dr. A. K. Pradhan, and Rajeh Mundle, Christian
Ezeagwu, Dexter Ezeagwu, Norfolk State University for their help in use
of the Four-point probe and UV-VIS-IR equipment, NASA Ames Research
Center, CA 94035 for TEM measurements, Jefferson Lab, Newport News, VA
23606 for FESEM and EDX measurements. The authors declare no competing
financial interest.
NR 35
TC 0
Z9 0
U1 3
U2 9
PU AMER SCIENTIFIC PUBLISHERS
PI VALENCIA
PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA
SN 1533-4880
EI 1533-4899
J9 J NANOSCI NANOTECHNO
JI J. Nanosci. Nanotechnol.
PD JAN
PY 2016
VL 16
IS 1
BP 1076
EP 1084
DI 10.1166/jnn.2016.10509
PG 9
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA DD1KK
UT WOS:000369680400142
PM 27398571
ER
PT J
AU Holmesparker, C
Agogino, AK
Tumer, K
AF Holmesparker, Chris
Agogino, Adrian K.
Tumer, Kagan
TI Combining reward shaping and hierarchies for scaling to large multiagent
systems
SO KNOWLEDGE ENGINEERING REVIEW
LA English
DT Article; Proceedings Paper
CT 2012 Adaptive and Learning Agents Workshop*
CY JUN 04-04, 2012
CL Valencia, SPAIN
AB Coordinating the actions of agents in multiagent systems presents a challenging problem, especially as the size of the system is increased and predicting the agent interactions becomes difficult. Many approaches to improving coordination within multiagent systems have been developed including organizational structures, shaped rewards, coordination graphs, heuristic methods, and learning automata. However, each of these approaches still have inherent limitations with respect to coordination and scalability. We explore the potential of synergistically combining existing coordination mechanisms such that they offset each others' limitations. More specifically, we are interested in combining existing coordination mechanisms in order to achieve improved performance, increased scalability, and reduced coordination complexity in large multiagent systems.
In this work, we discuss and demonstrate the individual limitations of two well-known coordination mechanisms. We then provide a methodology for combining the two coordination mechanisms to offset their limitations and improve performance over either method individually. In particular, we combine shaped difference rewards and hierarchical organization in the Defect Combination Problem with up to 10 000 sensing agents. We show that combining hierarchical organization with difference rewards can improve both coordination and scalability by decreasing information overhead, structuring agent-to-agent connectivity and control flow, and improving the individual decision-making capabilities of agents. We show that by combining hierarchies and difference rewards, the information overheads and computational requirements of individual agents can be reduced by as much as 99% while simultaneously increasing the overall system performance. Additionally, we demonstrate the robustness of this approach to handling up to 25% agent failures under various conditions.
C1 [Holmesparker, Chris; Tumer, Kagan] Oregon State Univ, Sch MIME, 442 Rogers Hall, Corvallis, OR 97331 USA.
[Agogino, Adrian K.] NASA Ames, UCSC, Mail Stop 269-3, Moffett Field, CA 94035 USA.
RP Holmesparker, C; Tumer, K (reprint author), Oregon State Univ, Sch MIME, 442 Rogers Hall, Corvallis, OR 97331 USA.; Agogino, AK (reprint author), NASA Ames, UCSC, Mail Stop 269-3, Moffett Field, CA 94035 USA.
EM holmespc@onid.orst.edu; Adrian.K.Agogino@nasa.gov;
kagan.tumer@oregonstate.edu
FU National Science Foundation [0931591]; National Energy Technology
Laboratory [DE-FE0000857]
FX This work was partially supported by the National Science Foundation
under grant 0931591 and the National Energy Technology Laboratory under
grant DE-FE0000857.
NR 30
TC 0
Z9 0
U1 2
U2 3
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0269-8889
EI 1469-8005
J9 KNOWL ENG REV
JI Knowl. Eng. Rev.
PD JAN
PY 2016
VL 31
IS 1
SI SI
BP 3
EP 18
DI 10.1017/S0269888915000156
PG 16
WC Computer Science, Artificial Intelligence
SC Computer Science
GA DE7YJ
UT WOS:000370852700002
ER
PT J
AU Abbott, BP
Abbott, R
Abbott, TD
Abernathy, MR
Acernese, F
Ackley, K
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Adya, VB
Affeldt, C
Agathos, M
Agatsuma, K
Aggarwal, N
Aguiar, OD
Ain, A
Ajith, P
Allen, B
Allocca, A
Altin, PA
Amariutei, DV
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, CC
Areeda, JS
Arnaud, N
Arun, KG
Ashton, G
Ast, M
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Baker, PT
Baldaccini, F
Ballardin, G
Ballmer, SW
Barayoga, JC
Barclay, SE
Barish, BC
Barker, D
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barta, D
Bartlett, J
Bartos, I
Bassiri, R
Basti, A
Batch, JC
Baune, C
Bavigadda, V
Bazzan, M
Behnke, B
Bejger, M
Belczynski, C
Bell, AS
Bell, CJ
Berger, BK
Bergman, J
Bergmann, G
Berry, CPL
Bersanetti, D
Bertolini, A
Betzwieser, J
Bhagwat, S
Bhandare, R
Bilenko, IA
Billingsley, G
Birch, J
Birney, R
Biscans, S
Bisht, A
Bitossi, M
Biwer, C
Bizouard, MA
Blackburn, JK
Blair, CD
Blair, D
Blair, RM
Bloernen, S
Bock, O
Bodiya, TP
Boer, M
Bogaert, G
Bogan, C
Bohe, A
Bojtos, P
Bond, C
Bondu, F
Bonnand, R
Bork, R
Boschi, V
Bose, S
Bozzi, A
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Briant, T
Brillet, A
Brinkmann, M
Brisson, V
Brockill, P
Brooks, AF
Brown, DA
Brown, DD
Brown, NM
Buchanan, CC
Buikema, A
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
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Cahillane, C
Bustillo, JC
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Camp, JB
Cannon, KC
Cao, J
Capano, CD
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Carbognani, F
Caride, S
Diaz, JC
Casentini, C
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Baiardi, LC
Cerretani, G
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chamberlin, SJ
Chan, M
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, HY
Chen, Y
Cheng, C
Chincarini, A
Chiummo, A
Cho, HS
Cho, M
Chow, JH
Christensen, N
Chu, Q
Chua, S
Chung, S
Ciani, G
Clara, F
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Coila, A
Collette, CG
Constancio, M
Conte, A
Conti, L
Cook, D
Corbitt, TR
Cornish, N
Corsi, A
Cortese, S
Costa, CA
Coughlin, MW
Coughlin, SB
Coulon, JP
Countryman, ST
Couvares, P
Coward, DM
Cowart, MJ
Coyne, DC
Coyne, R
Craig, K
Creighton, JDE
Cripe, J
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dal Canton, T
Danilishin, SL
D'Antonio, S
Danzmann, K
Darman, NS
Dattilo, V
Dave, I
Daveloza, HP
Davier, M
Davies, GS
Daw, EJ
Day, R
DeBra, D
Debreczeni, G
Degallaix, J
De Laurentis, M
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, R
De Rosa, R
DeSalvo, R
Dhurandhar, S
Diaz, MC
Di Fiore, L
Di Giovanni, M
Di Lieto, A
Di Palma, I
Di Virgilio, A
Dojcinoski, G
Dolique, V
Donovan, F
Dooley, KL
Doravari, S
Douglas, R
Downes, TP
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Ducrot, M
Dwyer, SE
Edo, TB
Edwards, MC
Effler, A
Eggenstein, HB
Ehrens, P
Eichholz, JM
Eikenberry, SS
Engels, W
Essick, RC
Etze, T
Evans, M
Evans, TM
Everett, R
Factourovich, M
Fafone, V
Fair, H
Fairhurst, S
Fan, X
Fang, Q
Farinon, S
Farr, B
Farr, WM
Favata, M
Fays, M
Fehrmann, H
Fejer, MM
Ferrante, I
Ferreira, EC
Ferrini, F
Fidecaro, F
Fiori, I
Fisher, RP
Flaminio, R
Fletcher, M
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Gabbard, HAG
Gair, JR
Garnrnaitoni, L
Gaonkar, SG
Garufi, F
Gatto, A
Gaur, G
Gehrels, N
Gemme, G
Gendre, B
Genin, E
Gennai, A
George, J
Gergely, L
Germain, V
Ghosh, A
Ghosh, S
Giaime, JA
Giardina, KD
Giazotto, A
Gill, K
Glaefke, A
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Castro, JMG
Gopakumar, A
Gordon, NA
Gorodetsky, ML
Gossan, SE
Gosselin, M
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greco, G
Green, AC
Groot, P
Grote, H
Grunewald, S
Guidi, GM
Guo, X
Gupta, A
Gupta, MK
Gushwa, KE
Gustafson, EK
Gustafson, R
Hacker, JJ
Hall, BR
Hall, ED
Hammond, G
Haney, M
Hanke, MM
Hanks, J
Hanna, C
Hannam, MD
Hanson, J
Hardwick, T
Harms, J
Harry, GM
Harry, IW
Hart, MJ
Hartman, MT
Haster, CJ
Haughian, K
Heidmann, A
Heintze, MC
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Hennig, J
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Hofman, D
Hollitt, SE
Holt, K
Holz, DE
Hopkins, P
Hosken, DJ
Hough, J
Houston, EA
Howell, EJ
Hu, YM
Huang, S
Huerta, EA
Huet, D
Hughey, B
Husa, S
Huttner, SH
Huynh-Dinh, T
Idrisy, A
Indik, N
Ingram, DR
Inta, R
Isa, HN
Isac, JM
Isi, M
Islas, G
Isogai, T
Iyer, BR
Izumi, K
Jacqmin, T
Jang, H
Jani, K
Jaranowski, P
Jawahar, S
Jimenez-Forteza, F
Johnson, WW
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalaghatgi, CV
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Karki, S
Kasprzack, M
Katsavounidis, E
Katzman, W
Kaufer, S
Kaur, T
Kawabe, K
Kawazoe, F
Kefelian, F
Kehl, MS
Keite, D
Kelley, DB
Kells, W
Kennedy, R
Key, JS
Khalaidovski, A
Khalili, FY
Khan, S
Khan, Z
Khazanov, EA
Kijbunchoo, N
Kim, C
Kirmo, J
Kina, K
Kim, N
Kim, N
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Kleybolte, L
Klimenko, S
Koehlenbeck, SM
Kokeyama, K
Koley, S
Kondrashov, V
Kontos, A
Korobko, M
Korth, WZ
Kowalska, I
Kozak, DB
Kringel, V
Krishnan, B
Krolak, A
Krueger, C
Kuehn, G
Kumar, P
Kuo, L
Kutynia, A
Lackey, BD
Landry, M
Lange, J
Lantz, B
Lasky, PD
Lazzarini, A
Lazzaro, C
Leaci, P
Leavey, S
Lebigot, E
Lee, CH
Lee, HK
Lee, HM
Lee, K
Lenon, A
Leonardi, M
Leong, JR
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Levin, Y
Levine, BM
Li, TGF
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Littenberg, TB
Lockerbie, NA
Logue, J
Lombardi, AL
Lord, JE
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, JD
Luck, H
Lundgren, AP
Luo, J
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Ma, Y
MacDonald, T
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Magee, RM
Mageswaran, M
Majorana, E
Maksimovic, I
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Mandel, I
Mandic, V
MaIlga, V
Mansell, GL
Manske, M
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, AS
Maros, E
Martelli, F
Martellini, L
Martin, IW
Martin, RM
Martynov, DV
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Masso-Reid, M
Matichard, F
Matone, L
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Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McCormick, S
McGuire, SC
McIntyre, G
McIver, J
McManus, DJ
McWilliams, ST
Meacher, D
Meadors, GD
Meidam, J
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Mendell, G
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Meshkov, S
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Meyers, PM
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Middleton, H
Mikhailov, EE
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Minenkov, Y
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Mishra, C
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
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Mohan, M
Mohapatra, SRP
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Moore, BC
Moore, CJ
Moraru, D
Moreno, G
Morriss, SR
Mossavi, K
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Mow-Lowry, CM
Mueller, CL
Mueller, G
Muir, AW
Mukherjee, A
Mukherjee, D
Mukherjee, S
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Murray, PG
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Nardecchia, I
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Newton, G
Nguyen, TT
Nielsen, AB
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Normandin, MEN
Nuttall, LK
Oberling, J
Ochsner, E
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Oh, JJ
Oh, SH
Ohme, F
Oliver, M
Oppermann, P
Oram, RJ
O'Reilly, B
O'Shaughnessy, R
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Overmier, H
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Pai, SA
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Paoli, A
Papa, MA
Paris, HR
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Pascucci, D
Pasqualetti, A
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Patrick, Z
Pearlstone, BL
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Pedurand, R
Pekowsky, L
Pele, A
Penn, S
Pereira, R
Perreca, A
Phelps, M
Piccinni, O
Pichot, M
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Poggiani, R
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Price, LR
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Purrer, M
Qi, H
Qin, J
Quetschke, V
Quintero, EA
Quitzow-James, R
Raab, FJ
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Radkins, H
Raffai, P
Raja, S
Rakhmanov, M
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Raymond, V
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Reed, CM
Regimbau, T
Rei, L
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van den Brand, J. F. J.
van den Broeck, C.
Vander-Hyde, D. C.
van der Schaaf, L.
van der Sluys, M. V.
van Heijningen, J. V.
van Veggel, A. A.
Vardaro, M.
Vass, S.
Vasuth, M.
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Vedovato, G.
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Vyatchanin, S. P.
Wade, A. R.
Wade, L. E.
Wade, M.
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Wallace, L.
Walsh, S.
Wang, G.
Wang, H.
Wang, M.
Wang, X.
Wang, Y.
Ward, R. L.
Warner, J.
Was, M.
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Wei, L. -W.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
Westphal, T.
Wette, K.
Whelan, J. T.
White, D. J.
Whiting, B. F.
Williams, R. D.
Williamson, A. R.
Willis, J. L.
Willke, B.
Wimmer, M. H.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Wright, J. L.
Wu, G.
Yablon, J.
Yam, W.
Yamamoto, H.
Yancey, C. C.
Yap, M. J.
Yu, H.
Yvert, M.
ZadroZny, A.
Zangrando, L.
Zanolin, M.
Zendri, J. -P.
Zevin, M.
Zhang, F.
Zhang, L.
Zhang, M.
Zhang, Y.
Zhao, C.
Zhou, M.
Zhou, Z.
Zhu, X. J.
Zucker, M. E.
Zuraw, S. E.
Zweizigl, J.
CA LIGO Sci Collaboration
LIGO Sci Collaboration
Virgo Collaboration
TI Prospects for Observing and Localizing Gravitational-Wave Transients
with Advanced LIGO and Advanced Virgo
SO LIVING REVIEWS IN RELATIVITY
LA English
DT Review
DE Gravitational waves; Gravitational-wave detectors; Electromagnetic
counterparts; Data analysis
ID ELECTROMAGNETIC COUNTERPARTS; FOLLOW-UP; PARAMETER-ESTIMATION; BINARY
COALESCENCE; CANDIDATE EVENTS; MERGER RATES; SEARCH; DETECTORS;
INSPIRALS
AB We present a possible observing scenario for the Advanced LIGO and Advanced Virgo gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We determine the expected sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron-star systems, which are considered the most promising for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90% credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5 deg(2) to 20 deg(2) will require at least three detectors of sensitivity within a factor of similar to 2 of each other and with a broad frequency bandwidth. Should the third LIGO detector be relocated to India as expected, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.
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[Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Giaime, J. A.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Kokeyama, K.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
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[Ackley, K.; Amariutei, D. V.; Ciani, G.; Eichholz, J. M.; Eikenberry, S. S.; Fulda, P.; Goetz, R.; Hartman, M. T.; Heintze, M. C.; Klimenko, S.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.] Univ Florida, Gainesville, FL 32611 USA.
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[Casentini, C.; Cesarini, E.; D'Antonio, S.; Fafone, V.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Re, V.; Rocchi, A.; Sequino, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Chao, S.; Cheng, C.; Huang, S.; Kuo, L.; Pan, H.] Natl Tsing Hua Univ, Hsinchu 30013, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, H. Y.; Farr, B.; Holz, D. E.] Univ Chicago, Chicago, IL 60637 USA.
[Chen, Y.; Engels, W.; Ott, C. D.; Schmidt, P.; Thorne, K. S.] Caltech CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Jang, H.; Kang, G.; Kim, C.; Kim, N.] Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea.
[Christensen, N.; Coughlin, M. W.; Edwards, M. C.; Luo, J.; Strauss, N. A.] Carleton Coll, Northfield, MN 55057 USA.
[Coccia, E.; Fafone, V.; Lorenzini, M.; Tiwari, S.; Wang, G.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Coila, A.; Conte, A.; Di Giovanni, M.; Frasca, S.; Leaci, P.; MaIlga, V.; Mezzani, F.; Naticchioni, L.; Piccinni, O.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Collette, C. G.] Univ Brussels, B-1050 Brussels, Belgium.
[Corsi, A.; Coyne, R.; Inta, R.; Owen, B. J.] Texas Tech Univ, Lubbock, TX 79409 USA.
[Coughlin, S. B.; Fairhurst, S.; Fays, M.; Hannam, M. D.; Hopkins, P.; Khan, S.; Muir, A. W.; Ohme, F.; Pannarale, F.; Predoi, V.; Puerrer, M.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Tiwari, V.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Crowder, S. G.; Mandic, V.; Meyers, P. M.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Darman, N. S.; Melatos, A.; Sammut, L.; Sun, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Daveloza, H. P.; Diaz, M. C.; Key, J. S.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Torres, C. V.; Tuyenbayev, D.; Valdes, G.] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA.
[Daw, E. J.; Edo, T. B.; Kennedy, R.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Favata, M.; Moore, B. C.] Montclair State Univ, Montclair, NJ 07043 USA.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Trento Inst Fundamental Phys & Applicat, Ist Nazl Fis Nucl, I-38123 Povo, Trento, Italy.
[Dojcinoski, G.; Everett, R.; Hanna, C.; Idrisy, A.; Messick, C.] Penn State Univ, University Pk, PA 16802 USA.
[Gair, J. R.; Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Gaur, G.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Gaur, G.; Gupta, M. K.; Khan, Z.; Srivastava, A. K.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary.
[Gill, K.; Hughey, B.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Hoak, D.; Lombardi, A. L.; McIver, J.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA.
[Hollitt, S. E.; Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Huerta, E. A.; McWilliams, S. T.] W Virginia Univ, Morgantown, WV 26506 USA.
[Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland.
[Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[Kalogera, V.; Littenberg, T. B.; Pankow, C.; Sandeen, B.; Shahriar, M. S.; Yablon, J.; Zevin, M.; Zhou, M.; Zhou, Z.] Northwestern Univ, Evanston, IL 60208 USA.
[Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kirmo, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Busan 609735, South Korea.
[Kina, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.; Kutynia, A.; ZadroZny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Lange, J.; O'Shaughnessy, R.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Lasky, P. D.; Levin, Y.; Premachandra, S. S.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil.
[Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[O'De, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Ogin, G. H.] Whitman Coll, 280 Boyer Ave, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Trozzo, L.] Univ Siena, Via Laterina 8, I-53100 Siena, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI De Laurentis, Martina/L-3022-2016; Pinto, Innocenzo/L-3520-2016; Groot,
Paul/K-4391-2016; Vecchio, Alberto/F-8310-2015; Graef,
Christian/J-3167-2015; Branchesi, Marica/P-2296-2015; Ferrante,
Isidoro/F-1017-2012; Chen, Yanbei/A-2604-2013; Garufi,
Fabio/K-3263-2015; McClelland, David/E-6765-2010; Losurdo,
Giovanni/K-1241-2014; Sorrentino, Fiodor/M-6662-2016; Travasso,
Flavio/J-9595-2016; Sergeev, Alexander/F-3027-2017; Harms,
Jan/J-4359-2012; Howell, Eric/H-5072-2014; Tiwari,
Shubhanshu/R-8546-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Danilishin, Stefan/K-7262-2012; Hild,
Stefan/A-3864-2010; Steinlechner, Sebastian/D-5781-2013; Chow,
Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Gammaitoni,
Luca/B-5375-2009; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora
Vittoria/E-9078-2015; Rocchi, Alessio/O-9499-2015; prodi,
giovanni/B-4398-2010; Gemme, Gianluca/C-7233-2008; Gorodetsky,
Michael/C-5938-2008; Strain, Kenneth/D-5236-2011; Strigin,
Sergey/I-8337-2012; Prokhorov, Leonid/I-2953-2012; Khalili,
Farit/D-8113-2012; Heidmann, Antoine/G-4295-2016; Bell,
Angus/E-7312-2011; Costa, Cesar/G-7588-2012; Puppo, Paola/J-4250-2012;
Iyer, Bala R./E-2894-2012; Nelemans, Gijs/D-3177-2012; Ott,
Christian/G-2651-2011; Piccinni, Ornella Juliana/C-1319-2016; Tacca,
Matteo/J-1599-2015; Leonardi, Matteo/G-9694-2015; Marchesoni,
Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi,
Franco/K-1068-2016; Vicere, Andrea/J-1742-2012; Sigg,
Daniel/I-4308-2015; Kumar, Prem/B-6691-2009; Lazzaro,
Claudia/L-2986-2016; Stratta, Maria Giuliana/L-3045-2016;
OI De Laurentis, Martina/0000-0002-3815-4078; Groot,
Paul/0000-0002-4488-726X; Vecchio, Alberto/0000-0002-6254-1617; Graef,
Christian/0000-0002-4535-2603; Ferrante, Isidoro/0000-0002-0083-7228;
Garufi, Fabio/0000-0003-1391-6168; McClelland,
David/0000-0001-6210-5842; Losurdo, Giovanni/0000-0003-0452-746X;
Sorrentino, Fiodor/0000-0002-9605-9829; Travasso,
Flavio/0000-0002-4653-6156; Vitale, Salvatore/0000-0003-2700-0767;
Berry, Christopher/0000-0003-3870-7215; Murphy,
David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Davies,
Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628;
Swinkels, Bas/0000-0002-3066-3601; Dolique, Vincent/0000-0001-5644-9905;
O'Shaughnessy, Richard/0000-0001-5832-8517; Howell,
Eric/0000-0001-7891-2817; Boschi, Valerio/0000-0001-8665-2293; Gatto,
Alberto/0000-0001-9090-983X; Tiwari, Shubhanshu/0000-0003-1611-6625;
Punturo, Michele/0000-0001-8722-4485; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Danilishin, Stefan/0000-0001-7758-7493; Steinlechner,
Sebastian/0000-0003-4710-8548; Chow, Jong/0000-0002-2414-5402; Frey,
Raymond/0000-0003-0341-2636; Gammaitoni, Luca/0000-0002-4972-7062;
Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Rocchi, Alessio/0000-0002-1382-9016;
prodi, giovanni/0000-0001-5256-915X; Gemme,
Gianluca/0000-0002-1127-7406; Gorodetsky, Michael/0000-0002-5159-2742;
Strain, Kenneth/0000-0002-2066-5355; Heidmann,
Antoine/0000-0002-0784-5175; Bell, Angus/0000-0003-1523-0821; Puppo,
Paola/0000-0003-4677-5015; Iyer, Bala R./0000-0002-4141-5179; Nelemans,
Gijs/0000-0002-0752-2974; Ott, Christian/0000-0003-4993-2055; Piccinni,
Ornella Juliana/0000-0001-5478-3950; Tacca, Matteo/0000-0003-1353-0441;
Marchesoni, Fabio/0000-0001-9240-6793; Zhu,
Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587;
Vicere, Andrea/0000-0003-0624-6231; Sigg, Daniel/0000-0003-4606-6526;
Lazzaro, Claudia/0000-0001-5993-3372; Stratta, Maria
Giuliana/0000-0003-1055-7980; Bondu, Francois/0000-0001-6487-5197;
Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; Gendre, Bruce/0000-0002-9077-2025; Granata,
Massimo/0000-0003-3275-1186; Papa, M.Alessandra/0000-0002-1007-5298;
Vocca, Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Guidi,
Gianluca/0000-0002-3061-9870; Collette, Christophe/0000-0002-4430-3703;
Addesso, Paolo/0000-0003-0895-184X; Naticchioni,
Luca/0000-0003-2918-0730; Scott, Jamie/0000-0001-6701-6515; Callister,
Thomas/0000-0001-9892-177X; Sorazu, Borja/0000-0002-6178-3198
FU Advanced LIGO; Science and Technology Facilities Council (STFC) of the
United Kingdom; Australian Research Council; Council of Scientific and
Industrial Research of India, Department of Science and Technology,
India; Science & Engineering Research Board (SERB), India; Ministry of
Human Resource Development, India; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia i Competitivitat and Conselleria
d'Educacio, Cultura i Universitats of the Govern de les Illes Balears;
National Science Centre of Poland; FOCUS Programme of Foundation for
Polish Science; European Union; Royal Society; Scottish Funding Council;
Scottish Universities Physics Alliance; Lyon Institute of Origins (LIO);
National Research Foundation of Korea; Industry Canada; Province of
Ontario through the Ministry of Economic Development and Innovation;
National Science and Engineering Research Council Canada; Brazilian
Ministry of Science, Technology, and Innovation; Research Corporation,
Ministry of Science and Technology (MOST), Taiwan; Kavli Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation (NSF) for the construction and operation of
the LIGO Laboratory and Advanced LIGO as well as the Science and
Technology Facilities Council (STFC) of the United Kingdom, the
Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for
support of the construction of Advanced LIGO and construction and
operation of the GEO600 detector. Additional support for Advanced LIGO
was provided by the Australian Research Council. The authors gratefully
acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN),
the French Centre National de la Recherche Scientifique (CNRS) and the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, for the construction
and operation of the Virgo detector and the creation and support of the
EGO consortium. The authors also gratefully acknowledge research support
from these agencies as well as by the Council of Scientific and
Industrial Research of India, Department of Science and Technology,
India, Science & Engineering Research Board (SERB), India, Ministry of
Human Resource Development, India, the Spanish Ministerio de Economia y
Competitividad, the Conselleria d'Economia i Competitivitat and
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears, the National Science Centre of Poland, the FOCUS
Programme of Foundation for Polish Science, the European Union, the
Royal Society, the Scottish Funding Council, the Scottish Universities
Physics Alliance, the Lyon Institute of Origins (LIO), the National
Research Foundation of Korea, Industry Canada and the Province of
Ontario through the Ministry of Economic Development and Innovation, the
National Science and Engineering Research Council Canada, the Brazilian
Ministry of Science, Technology, and Innovation, the Research
Corporation, Ministry of Science and Technology (MOST), Taiwan and the
Kavli Foundation. The authors gratefully acknowledge the support of the
NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for
provision of computational resources.
NR 113
TC 78
Z9 77
U1 27
U2 79
PU SPRINGER INTERNATIONAL PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 1433-8351
J9 LIVING REV RELATIV
JI Living Rev. Relativ.
PY 2016
VL 19
BP 1
EP +
DI 10.1007/lrr-2016-1
PG 38
WC Physics, Particles & Fields
SC Physics
GA DD7RZ
UT WOS:000370123100001
PM 28179853
ER
PT J
AU Limoli, C
Baulch, J
Sowa, M
AF Limoli, Charles
Baulch, Janet
Sowa, Marianne
TI William F. Morgan (1952-2015) IN MEMORIAM
SO RADIATION RESEARCH
LA English
DT Biographical-Item
C1 [Limoli, Charles; Baulch, Janet] Univ Calif Irvine, Irvine, CA USA.
[Sowa, Marianne] NASA, Ames Res Ctr, Washington, DC USA.
RP Limoli, C (reprint author), Univ Calif Irvine, Irvine, CA USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
EI 1938-5404
J9 RADIAT RES
JI Radiat. Res.
PD JAN
PY 2016
VL 185
IS 1
BP 106
EP 108
DI 10.1667/RR00WM.1
PG 3
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA DE6IK
UT WOS:000370737000013
PM 26789848
ER
PT J
AU Lang, R
Zhou, YW
Utku, C
Le Vine, D
AF Lang, Roger
Zhou, Yiwen
Utku, Cuneyt
Le Vine, David
TI Accurate measurements of the dielectric constant of seawater at L band
SO RADIO SCIENCE
LA English
DT Article
DE seawater dielectric measurement; L band; microwave cavity; seawater
salinity
ID PERMITTIVITY MEASUREMENTS; MICROWAVE-FREQUENCIES; COMPLEX PERMITTIVITY;
LIQUID WATER; SEA-WATER; MODEL; SALINITY; SURFACE; RANGE; GHZ
AB This paper describes measurements of the dielectric constant of seawater at a frequency of 1.413GHz, the center of the protected band (i.e., passive use only) used in the measurement of sea surface salinity from space. The objective of the measurements is to accurately determine the complex dielectric constant of seawater as a function of salinity and temperature. A resonant cylindrical microwave cavity in transmission mode has been employed to make the measurements. The measurements are made using standard seawater at salinities of 30, 33, 35, and 38 practical salinity units over a range of temperatures from 0 degrees C to 35 degrees C in 5 degrees C intervals. Repeated measurements have been made at each temperature and salinity. Mean values and standard deviations are then computed. The total error budget indicates that the real and imaginary parts of the dielectric constant have a combined standard uncertainty of about 0.3 over the range of salinities and temperatures considered. The measurements are compared with the dielectric constants obtained from the model functions of Klein and Swift and those of Meissner and Wentz. The biggest differences occur at low and high temperatures.
C1 [Lang, Roger; Zhou, Yiwen] George Washington Univ, Dept Elect & Comp Engn, Washington, DC USA.
[Utku, Cuneyt] Prime Minist Sci & Technol Directorate, Ankara, Turkey.
[Le Vine, David] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab Code 615, Greenbelt, MD USA.
RP Lang, R (reprint author), George Washington Univ, Dept Elect & Comp Engn, Washington, DC USA.
EM lang@gwu.edu
FU NASA [NNX09AU72G]
FX The data generated from these measurements are contained in the
supporting information. The data in this file were used to generate the
data plots and data tables listed in the paper. The work on the project
was supported by NASA grant NNX09AU72G. The authors would like to thank
Jerzy Krupka of the Warsaw University of Technology in Warsaw, Poland,
for helping with the initial design of the cavity and James Baker-Jarvis
and Michael Janezic of National Institute of Standards and Technology
(NIST) for the advice that they have given. We would like to thank
Thomas Manuccia who advised Jared Janiczek in the construction of the
control and automation systems for his senior project at the George
Washington University (GW). We also would like to thank Yalcin Tarkocin
for performing the initial set of measurements in 2007-2008.
NR 33
TC 1
Z9 1
U1 4
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD JAN
PY 2016
VL 51
IS 1
BP 2
EP 24
DI 10.1002/2015RS005776
PG 23
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA DE5CX
UT WOS:000370649700001
ER
PT J
AU Li, F
Choudhari, M
Carpenter, M
Malik, M
Chang, CL
Streett, C
AF Li, Fei
Choudhari, Meelan
Carpenter, Mark
Malik, Mujeeb
Chang, Chau-Lyan
Streett, Craig
TI Control of Crossflow Transition at High Reynolds Numbers Using Discrete
Roughness Elements
SO AIAA JOURNAL
LA English
DT Article
ID 3-DIMENSIONAL BOUNDARY-LAYERS; DIRECT NUMERICAL-SIMULATION; SECONDARY
INSTABILITY; PASSIVE CONTROL; VORTICES
AB Transition analysis is performed for a swept wing at a Mach number of 0.75 and chord Reynolds number of approximately 1.7x10(7), with a focus on roughness-based crossflow-transition control at high Reynolds numbers relevant to subsonic flight. The roughness-based transition control involves controlled seeding of suitable, subdominant crossflow modes to weaken the growth of naturally occurring, linearly more unstable instability modes via a nonlinear modification of the mean boundary-layer profiles. Therefore, a synthesis of receptivity, linear and nonlinear growth of crossflow disturbances, and high-frequency secondary instabilities becomes desirable to model this form of control. Because experimental data are currently unavailable for passive crossflow-transition control on high-Reynolds-number configurations, a holistic computational approach is used to assess the feasibility of roughness-based-control methodology. The potential challenges inherent to this control application, as well as the associated difficulties in modeling this form of control in a computational setting, are highlighted. At high Reynolds numbers, a broad spectrum of stationary-crossflow disturbances have large-enough linear amplification to cause transition, and, while it may be possible to control a specific target mode using discrete roughness elements, the nonlinear interaction between the control and target modes may yield strong amplification of the difference mode and, hence, produce an adverse impact on the transition delay using spanwise periodic roughness elements.
C1 [Li, Fei; Choudhari, Meelan; Carpenter, Mark; Malik, Mujeeb; Chang, Chau-Lyan; Streett, Craig] NASA, Langley Res Ctr, Computat AeroSci Branch, MS128, Hampton, VA 23681 USA.
RP Li, F; Choudhari, M; Carpenter, M; Malik, M; Chang, CL; Streett, C (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, MS128, Hampton, VA 23681 USA.
EM fei.li@nasa.gov; meelan.m.choudhari@nasa.gov; mark.h.carpenter@nasa.gov;
mujeeb.r.malik@nasa.gov; chau-lyan.chang@nasa.gov;
craig.l.strreett@nasa.gov
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
FU NASA's Subsonic Fixed Wing; Aeronautical Sciences; NASA's Subsonic Fixed
Wing project; Aeronautical Sciences project; Environmentally Responsible
Aviation project
FX The present work is part of a collaborative effort with W. S. Saric and
his research group at Texas A&M University (TAMU). Technical
interactions with the TAMU team are gratefully acknowledged. The authors
also thank Michael Belisle from TAMU for providing the design data
associated with the wing configuration studied herein. This work was
performed in support of NASA's Subsonic Fixed Wing, Aeronautical
Sciences, and the Environmentally Responsible Aviation projects.
NR 24
TC 1
Z9 1
U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2016
VL 54
IS 1
BP 39
EP 52
DI 10.2514/1.J054067
PG 14
WC Engineering, Aerospace
SC Engineering
GA DD6TE
UT WOS:000370056600003
ER
PT J
AU Watkins, AN
Leighty, BD
Lipford, WE
Goodman, KZ
Crafton, J
Gregory, JW
AF Watkins, A. Neal
Leighty, Bradley D.
Lipford, William E.
Goodman, Kyle Z.
Crafton, Jim
Gregory, James W.
TI Measuring Surface Pressures on Rotor Blades Using Pressure-Sensitive
Paint
SO AIAA JOURNAL
LA English
DT Article
ID FILM-COOLING EFFECTIVENESS; TURBINE BLADE
AB This paper will present details of a pressure-sensitive paint system for measuring global surface pressures on rotor blades in simulated forward flight at the 14x22 ft subsonic tunnel at the NASA Langley Research Center. The system was designed to use a pulsed laser as an excitation source and pressure-sensitive paint data were collected using the lifetime-based approach. The higher intensity of the laser allowed pressure-sensitive paint images to be acquired using a single laser pulse, resulting in a collection of images that can be used to determine blade pressure at a specific instant in time. This is extremely important in rotorcraft applications because the blades experience dramatically different flowfields depending on their position. In addition, there can be fluctuations on the blade that vary every cycle due to factors such as lead/lag, flapping, and twisting of the blade. These effects generally preclude the use of phase averaging and thus the need for acquiring the data in a single image pair. For this test, the entire upper surface of a blade was painted and imaged. After taking into account temperature effects on the pressure-sensitive paint, the results agree both qualitatively and quantitatively with both expected results as well as with pressure transducers. Several limitations of the technique have been identified and discussion of strategies to overcome them is also presented.
C1 [Watkins, A. Neal; Leighty, Bradley D.; Lipford, William E.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23669 USA.
[Watkins, A. Neal; Goodman, Kyle Z.] Analyt Mech Associates Inc, Adv Sensing & Optic Measurement Branch, Mail Stop 493, Hampton, VA 23669 USA.
[Crafton, Jim] Innovat Sci Solut Inc, 7610 McEwen Rd, Dayton, OH 45459 USA.
[Gregory, James W.] Ohio State Univ, Aerosp Res Ctr, Dept Mech & Aerosp Engn, 2300 West Case Road, Columbus, OH 43235 USA.
RP Watkins, AN (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23669 USA.; Watkins, AN (reprint author), Analyt Mech Associates Inc, Adv Sensing & Optic Measurement Branch, Mail Stop 493, Hampton, VA 23669 USA.
RI Gregory, James/A-2343-2015
OI Gregory, James/0000-0002-8589-8758
FU Rotary Wing project under the NASA Fundamental Aeronautics Program; NASA
Phase I Small Business Innovation Research grant [NNX12CD07P]; Sierra
Lobo, Inc.
FX This work was funded by the Rotary Wing project under the NASA
Fundamental Aeronautics Program, as well as NASA Phase I Small Business
Innovation Research grant NNX12CD07P. The authors wish to thank Oliver
Wong, Preston Martin, Philip Tanner, Austin Overmeyer, and Bryan Mann
from the U.S. Army Aeroflightdynamics and Derry Mace from Sierra Lobo,
Inc. for their support during this program, and the entire staff of the
14 x 22 ft subsonic tunnel for their assistance and support during the
wind-tunnel entry. The authors also gratefully acknowledge Susan Gorton,
the Principal Investigator for the Rotary Wing project, who has
continued to support and encourage this work since its inception.
NR 32
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2016
VL 54
IS 1
BP 206
EP 215
DI 10.2514/1.J054191
PG 10
WC Engineering, Aerospace
SC Engineering
GA DD6TE
UT WOS:000370056600016
ER
PT J
AU Guo, YP
Thomas, RH
AF Guo, Yueping
Thomas, Russell H.
TI Experimental Study on Open Rotor Noise Shielding by Hybrid-Wing-Body
Aircraft
SO AIAA JOURNAL
LA English
DT Article
AB This paper presents an experimental study on open rotor noise shielding by hybrid-wing-body aircraft, with the objective of understanding the noise shielding features and establishing methods of applying the shielding data for system noise studies of hybrid-wing-body aircraft. By studying the directivity patterns of individual tones, it is shown that, although the tonal energy distribution and the spectral content of the wind-tunnel test model (and thus its total noise) may differ from those of more advanced rotor designs, the individual tones follow directivity patterns that characterize far-field radiations of modern open rotors, establishing the validity of the use of this shielding database, provided that the shielding effects are applied on individual tones. To this end, open rotor tonal noise shielding is categorized into front rotor tones, aft rotor tones, and interaction tones: not only because of their different directivities but also due to the differences in their source locations and coherence features, which make their respective shielding characteristics distinctly different from each other. To reveal the parametric trends of the hybrid-wing-body shielding effects, results are presented with variations in frequency, far-field emission angle, rotor operational condition, engine installation, and local airframe features.
C1 [Guo, Yueping] Boeing Co, Huntington Beach, CA 92647 USA.
[Thomas, Russell H.] NASA, Langley Res Ctr, Aeroacoust Branch, Mail Stop 461, Hampton, VA 23681 USA.
[Guo, Yueping] NEAT Consulting, 3830 Daisy Circle, Seal Beach, CA 90740 USA.
RP Guo, YP (reprint author), Boeing Co, Huntington Beach, CA 92647 USA.; Guo, YP (reprint author), NEAT Consulting, 3830 Daisy Circle, Seal Beach, CA 90740 USA.
FU Fay Collier as the Project Manager
FX The authors thank the NASA Environmentally Responsible Aviation Project,
with Fay Collier as the Project Manager, for funding this research.
NR 6
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U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2016
VL 54
IS 1
BP 242
EP 253
DI 10.2514/1.J054243
PG 12
WC Engineering, Aerospace
SC Engineering
GA DD6TE
UT WOS:000370056600019
ER
PT J
AU Stanford, BK
Jutte, CV
Wieseman, CD
AF Stanford, Bret K.
Jutte, Christine V.
Wieseman, Carol D.
TI Trim and Structural Optimization of Subsonic Transport Wings Using
Nonconventional Aeroelastic Tailoring
SO AIAA JOURNAL
LA English
DT Article
ID FUNCTIONALLY GRADED MATERIALS; COMPOSITE WINGS; CONSTRAINTS; DESIGN;
PANELS
AB Several minimum-mass aeroelastic optimization problems are solved to evaluate the effectiveness of a variety of novel tailoring schemes for subsonic transport wings. Aeroelastic strength and panel buckling constraints are imposed across several trimmed maneuver loads, in addition to flutter constraints. Tailoring with metallic thickness variations, functionally graded materials, composite laminates, tow steering within composite laminates, and distributed trailing-edge control effectors are all found to provide reductions in structural wing mass with varying degrees of success. The question as to whether this wing mass reduction will offset the increased manufacturing cost is left unresolved for each case.
C1 [Stanford, Bret K.; Wieseman, Carol D.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
[Jutte, Christine V.] Craig Technol Inc, Adv Mat & Proc Branch, Cape Canaveral, FL 32920 USA.
RP Stanford, BK; Wieseman, CD (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.; Jutte, CV (reprint author), Craig Technol Inc, Adv Mat & Proc Branch, Cape Canaveral, FL 32920 USA.
EM bret.k.stanford@nasa.gov; christine.v.jutte@nasa.gov;
carol.d.wieseman@nasa.gov
FU NASA's Advanced Air Transport Technologies program
FX This work is funded by NASA's Advanced Air Transport Technologies
program.
NR 32
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U1 1
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2016
VL 54
IS 1
BP 293
EP 309
DI 10.2514/1.J054244
PG 17
WC Engineering, Aerospace
SC Engineering
GA DD6TE
UT WOS:000370056600023
ER
PT J
AU Miller, SAE
AF Miller, Steven A. E.
TI Prediction of Scattered Broadband Shock-Associated Noise
SO AIAA JOURNAL
LA English
DT Article
ID EXPANDED SUPERSONIC JETS; ACOUSTIC ANALOGY; MIXING NOISE; FLAT-PLATE;
MODEL; TURBULENCE; SCHEMES
AB A mathematical model is developed for the prediction of broadband shock-associated noise in the presence of an airframe body. Model arguments are dependent on the vector Green's function of the linearized Euler equations, steady Reynolds-averaged Navier-Stokes solutions, and the two-point cross-correlation of the equivalent source. The equivalent source is dependent on steady Reynolds-averaged Navier-Stokes solutions of the jet flow that capture the nozzle and airframe geometry. Contours of the time-averaged streamwise velocity component and turbulent kinetic energy are examined with varying airframe position relative to the nozzle exit. Propagation effects are incorporated by approximating the vector Green's function of the linearized Euler equations. This approximation involves the use of ray theory and an assumption that broadband shock-associated noise is relatively unaffected by the refraction of the jet shear layer. A nondimensional parameter is proposed that quantifies the changes of the broadband shock-associated noise source with varying jet operating condition and airframe position. Scattered broadband shock-associated noise possesses a second set of broadband lobes that are due to the effect of scattering. Presented predictions from an overexpanded jet demonstrate relatively good agreement compared to a wide variety of measurements.
C1 [Miller, Steven A. E.] NASA, Langley Res Ctr, Aeroacoust Branch, 2 North Dryden St,MS 461, Hampton, VA 23681 USA.
RP Miller, SAE (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, 2 North Dryden St,MS 461, Hampton, VA 23681 USA.
EM s.miller@nasa.gov
NR 41
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U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2016
VL 54
IS 1
BP 343
EP 359
DI 10.2514/1.J054280
PG 17
WC Engineering, Aerospace
SC Engineering
GA DD6TE
UT WOS:000370056600027
ER
PT J
AU Lopez, DH
Rabbani, MR
Crosbie, E
Raman, A
Arellano, AF
Sorooshian, A
AF Lopez, David H.
Rabbani, Michael R.
Crosbie, Ewan
Raman, Aishwarya
Arellano, Avelino F., Jr.
Sorooshian, Armin
TI Frequency and Character of Extreme Aerosol Events in the Southwestern
United States: A Case Study Analysis in Arizona
SO ATMOSPHERE
LA English
DT Article
DE aerosol; dust; IMPROVE; Asian dust; Arizona; air quality; extreme events
ID ASIAN DUST EVENT; FORECAST MODEL; NORTH-AMERICA; AIR-POLLUTION; APRIL
1998; TRENDS; US; PROJECTIONS; SATELLITE; WILDFIRES
AB This study uses more than a decade's worth of data across Arizona to characterize the spatiotemporal distribution, frequency, and source of extreme aerosol events, defined as when the concentration of a species on a particular day exceeds that of the average plus two standard deviations for that given month. Depending on which of eight sites studied, between 5% and 7% of the total days exhibited an extreme aerosol event due to either extreme levels of PM10, PM2.5, and/or fine soil. Grand Canyon exhibited the most extreme event days (120, i.e., 7% of its total days). Fine soil is the pollutant type that most frequently impacted multiple sites at once at an extreme level. PM10, PM2.5, fine soil, non-Asian dust, and Elemental Carbon extreme events occurred most frequently in August. Nearly all Asian dust extreme events occurred between March and June. Extreme Elemental Carbon events have decreased as a function of time with statistical significance, while other pollutant categories did not show any significant change. Extreme events were most frequent for the various pollutant categories on either Wednesday or Thursday, but there was no statistically significant difference in the number of events on any particular day or on weekends versus weekdays.
C1 [Lopez, David H.; Rabbani, Michael R.; Sorooshian, Armin] Univ Arizona, Dept Chem & Environm Engn, Tucson, AZ 85721 USA.
[Crosbie, Ewan] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA.
[Crosbie, Ewan] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Raman, Aishwarya; Arellano, Avelino F., Jr.; Sorooshian, Armin] Univ Arizona, Dept Hydrol & Atmospher Sci, Tucson, AZ 85721 USA.
RP Sorooshian, A (reprint author), Univ Arizona, Dept Chem & Environm Engn, Tucson, AZ 85721 USA.; Sorooshian, A (reprint author), Univ Arizona, Dept Hydrol & Atmospher Sci, Tucson, AZ 85721 USA.
EM davidlopez3@email.arizona.edu; michaelrabbani@email.arizona.edu;
ewan.c.crosbie@nasa.gov; aishwaryaraman@email.arizona.edu;
arellano@atmo.arizona.edu; armin@email.arizona.edu
OI Sorooshian, Armin/0000-0002-2243-2264
FU National Institute of Environmental Health Sciences (NIEHS) Superfund
Research Program, NIH [2 P42 ES04940-11]; Center for Environmentally
Sustainable Mining through the TRIF Water Sustainability Program at the
University of Arizona
FX This work was funded by Grant 2 P42 ES04940-11 from the National
Institute of Environmental Health Sciences (NIEHS) Superfund Research
Program, NIH and the Center for Environmentally Sustainable Mining
through the TRIF Water Sustainability Program at the University of
Arizona. The authors acknowledge Andrew Huerta and the UROC-PREP program
in the Graduate College at the University of Arizona. The authors
gratefully acknowledge data provided by EPA IMPROVE and the NRL NAAPS
model. Some of the analyses and visualizations used in this study were
produced with the Giovanni online data system, developed and maintained
by the NASA GES DISC.
NR 43
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U1 0
U2 4
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2073-4433
J9 ATMOSPHERE-BASEL
JI Atmosphere
PD JAN
PY 2016
VL 7
IS 1
DI 10.3390/atmos7010001
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3QL
UT WOS:000369837500001
ER
PT J
AU Berry, C
Hill, RL
Walker, BK
AF Berry, Charlotte
Hill, Ronald L.
Walker, Brian K.
TI Demographics of a nearshore mating queen conch (Lobatus gigas)
aggregation on the southeast Florida Reef Tract
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article
ID STROMBUS-GIGAS; SEAGRASS MEADOWS; GASTROPOD; MARINE; KEYS; AGE
AB The queen conch, Lobatus gigas (Linnaeus, 1758), is a large gastropod found throughout the Caribbean region, including off Florida. The extent, habitat association, and population demographics of an aggregation were investigated off southeast Florida near a major shipping port. Population surveys were conducted over 4 km(2) of hard-bottom habitats to document benthic cover, conch distribution, and size data within 2 km north and south of the shipping inlet. In total, 122 conch were recorded for the entire surveyed area, equating to 70.6 conch ha(-1). Mean density was highest south of the inlet. Juvenile and subadult conch were found throughout the study area, but mostly in the westernmost, shallowest hard-bottom habitats. The highest density of adult conch was found in the CPW south of the inlet. Analyses showed that CPW south has a unique community composition dominated by macroalgae and sand. This area was surveyed further using cross-shelf transects measuring conch extent and demographics. Five-hundred and-twenty-five conch were found, resulting in a density of 495 ha(-1). Confirmed mating sightings, females with eggs, and solitary egg masses were found indicating reproduction in this nearshore habitat is successful. The ratio of females with eggs to those without indicated that, although 21.2% of the females with eggs had a thinner lip, the majority had a lip thickness >12 mm. Nearshore mating conch should be a consideration in beach construction projects. Future research should include reconnaissance for other aggregations, monitoring, and comparisons among other nearshore populations.
C1 [Berry, Charlotte; Walker, Brian K.] Nova SE Univ, Halmos Coll Nat Sci & Oceanog, GIS & Spatial Ecol Lab, Dania, FL 33004 USA.
[Hill, Ronald L.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston, TX 77551 USA.
RP Walker, BK (reprint author), Nova SE Univ, Halmos Coll Nat Sci & Oceanog, GIS & Spatial Ecol Lab, Dania, FL 33004 USA.
EM walkerb@nova.edu
NR 29
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U1 6
U2 8
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
EI 1553-6955
J9 B MAR SCI
JI Bull. Mar. Sci.
PD JAN
PY 2016
VL 92
IS 1
BP 59
EP 73
DI 10.5343/bms.2015.1047
PG 15
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA DD7OJ
UT WOS:000370113700005
ER
PT J
AU Gravelle, CM
Mecikalski, JR
Line, WE
Bedka, KM
Petersen, RA
Sieglaff, JM
Stano, GT
Goodman, SJ
AF Gravelle, Chad M.
Mecikalski, John R.
Line, William E.
Bedka, Kristopher M.
Petersen, Ralph A.
Sieglaff, Justin M.
Stano, Geoffrey T.
Goodman, Steven J.
TI DEMONSTRATION OF A GOES-R SATELLITE CONVECTIVE TOOLKIT TO "BRIDGE THE
GAP" BETWEEN SEVERE WEATHER WATCHES AND WARNINGS An Example from the 20
May 2013 Moore, Oklahoma, Tornado Outbreak
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID VHF RADIO PICTURES; BASE-LINE IMAGER; REAL-TIME; STORM INITIATION;
SYSTEM; THUNDERSTORM; ALGORITHM; MODEL; RADAR; EVOLUTION
AB With the launch of the Geostationary Operational Environmental Satellite-R (GOES-R) series in 2016, there will be continuity of observations for the current GOES system operating over the Western Hemisphere. The GOES-R Proving Ground was established in 2008 to help prepare satellite user communities for the enhanced capabilities of GOES-R, including new instruments, imagery, and products that will have increased spectral, spatial, and temporal resolution. This is accomplished through demonstration and evaluation of proxy products that use current GOES data, higher-resolution data provided by polar-orbiting satellites, and model-derived synthetic satellite imagery. The GOES-R demonstration products presented here, made available to forecasters in near-real time (within 20 min) via the GOES-R Proving Ground, include the 0-9-h NearCast model, 0-1-h convective initiation probabilities, convective cloud-top cooling, overshooting top detection, and a pseudo-Geostationary Lightning Mapper total lightning tendency diagnostic. These products are designed to assist in identifying areas of increasing convective instability, pre-radar echo cumulus cloud growth preceding thunderstorm formation, storm updraft intensity, and potential storm severity derived from lightning trends. In turn, they provide the warning forecaster with improved situational awareness and short-term predictive information that enhance their ability to monitor atmospheric conditions preceding and associated with the development of deep convection, a time period that typically occurs between the issuance of National Weather Service (NWS) Storm Prediction Center convective watches and convective storm warnings issued by NWS forecast offices. This paper will focus on how this GOES-R satellite convective toolkit could have been used by warning forecasters to enhance near-storm environment analysis and the warning-decision-making process prior to and during the 20 May 2013 Moore, Oklahoma, tornado event.
C1 [Gravelle, Chad M.] NOAA NWS Operat Proving Ground, 7220 NW 101st Terr, Kansas City, MO 64153 USA.
[Gravelle, Chad M.; Petersen, Ralph A.; Sieglaff, Justin M.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
[Mecikalski, John R.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
[Line, William E.] Univ Oklahoma, NOAA NWS Storm Predict Ctr, Norman, OK 73019 USA.
[Line, William E.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA.
[Bedka, Kristopher M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Stano, Geoffrey T.] NASA, Short Term Predict Res & Transit Ctr, Huntsville, AL USA.
[Stano, Geoffrey T.] ENSCO Inc, Huntsville, AL USA.
[Goodman, Steven J.] NASA, Goddard Space Flight Ctr, GOES R Program Off, Greenbelt, MD USA.
[Goodman, Steven J.] NOAA, Natl Environm Satellite Data & Informat Serv, Greenbelt, MD USA.
RP Gravelle, CM (reprint author), NOAA NWS Operat Proving Ground, 7220 NW 101st Terr, Kansas City, MO 64153 USA.; Gravelle, CM (reprint author), Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
EM chad.gravelle@noaa.gov
FU NOAA/STAR GOES-R Proving Ground grant; GOES Improved Measurements and
Products Activities Plan grant under NOAA-University of Wisconsin, U.S.
Department of Commerce [NA10NES440001]; NOAA, U.S. Department of
Commerce [NA11NES4400014]; NOAA GOES-R Algorithm Working Group Grant,
U.S. Department of Commerce [NA06NES4400002]
FX The authors thank Steven Weiss (NOAA/NWS/Storm Prediction Center), Dave
Radell (NOAA/NWS, Eastern Region Headquarters), Jeffrey Craven
(NOAA/NWS, Milwaukee/Sullivan, Wisconsin), and Frank Alsheimer
(NOAA/NWS, Charleston, South Carolina) for their reviews of earlier
versions of this manuscript and the three anonymous reviewers and the
journal editor, who provided thorough comments that improved the final
version of this paper. Funding is supported by a NOAA/STAR GOES-R
Proving Ground grant; a GOES Improved Measurements and Products
Activities Plan grant under NOAA-University of Wisconsin Cooperative
Agreement NA10NES440001, the U.S. Department of Commerce; NOAA Grant
NA11NES4400014, U.S. Department of Commerce; and NOAA GOES-R Algorithm
Working Group Grant NA06NES4400002, U.S. Department of Commerce.
NR 66
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U1 1
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2016
VL 97
IS 1
BP 69
EP 84
DI 10.1175/BAMS-D-14-00054.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD6WW
UT WOS:000370066300001
ER
PT J
AU Bodeker, GE
Bojinski, S
Cimini, D
Dirksen, RJ
Haeffelin, M
Hannigan, JW
Hurst, DF
Leblanc, T
Madonna, F
Maturilli, M
Mikalsen, AC
Philipona, R
Reale, T
Seidel, DJ
Tan, DGH
Thorne, PW
Vomel, H
Wang, J
AF Bodeker, G. E.
Bojinski, S.
Cimini, D.
Dirksen, R. J.
Haeffelin, M.
Hannigan, J. W.
Hurst, D. F.
Leblanc, T.
Madonna, F.
Maturilli, M.
Mikalsen, A. C.
Philipona, R.
Reale, T.
Seidel, D. J.
Tan, D. G. H.
Thorne, P. W.
Voemel, H.
Wang, J.
TI REFERENCE UPPER-AIR OBSERVATIONS FOR CLIMATE From Concept to Reality
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID RADIOSONDE; VALIDATION; PRODUCTS; NETWORK
C1 [Bodeker, G. E.] Bodeker Sci, 42 Russell St, Alexandra 9320, New Zealand.
[Bojinski, S.] World Meteorol Org, Space Programme, Geneva, Switzerland.
[Cimini, D.; Madonna, F.] CNR, Ist Metodol Anal Ambientale, Potenza, Italy.
[Cimini, D.] Univ Aquila, Ctr Eccellenza Telerilevamento & Modellist Numer, I-67100 Laquila, Italy.
[Dirksen, R. J.; Voemel, H.] Deutsch Wetterdienst, Lindenberg Meteorol Observ, Lindenberg, Germany.
[Haeffelin, M.] CNRS, Inst Pierre Simon Laplace, Paris, France.
[Hannigan, J. W.] Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA.
[Hurst, D. F.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Hurst, D. F.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA.
[Leblanc, T.] CALTECH, Jet Prop Lab, Wrightwood, CA USA.
[Maturilli, M.] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Potsdam, Germany.
[Mikalsen, A. C.] Nansen Environm & Remote Sensing Ctr, Bergen, Norway.
[Philipona, R.] Fed Off Meteorol & Climatol MeteoSwiss, Payerne, Switzerland.
[Reale, T.] NOAA, Ctr Satellite Applicat & ResCtr Satellite Applica, College Pk, MD USA.
[Seidel, D. J.] NOAA, Air Resources Lab, College Pk, MD USA.
[Tan, D. G. H.] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
[Thorne, P. W.] Maynooth Univ, Dept Geog, Maynooth, Kildare, Ireland.
[Wang, J.] SUNY Albany, Albany, NY 12222 USA.
RP Bodeker, GE (reprint author), Bodeker Sci, 42 Russell St, Alexandra 9320, New Zealand.
EM greg@bodekerscientific.com
RI Reale, Tony/F-5621-2010; Thorne, Peter/F-2225-2014;
OI Reale, Tony/0000-0003-2150-5246; Thorne, Peter/0000-0003-0485-9798;
Bodeker, Gregory/0000-0003-1094-5852
FU National Aeronautics and Space Administration
FX Part of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 31
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U1 1
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2016
VL 97
IS 1
BP 123
EP 135
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD6WZ
UT WOS:000370066600001
ER
PT J
AU Deshpande, AD
Dockum, BW
Draxler, AFJ
AF Deshpande, Ashok D.
Dockum, Bruce W.
Draxler, Andrew F. J.
TI Contaminant bioaccumulation dynamics in young-of-the-year bluefish
subpopulations in New York Bight with a special reference to the
condition and nursery area fidelity subsequent to recruitment
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID REPRODUCTIVE BIOMARKER RESPONSES; POMATOMUS-SALTATRIX; UNITED-STATES;
POLYCHLORINATED-BIPHENYLS; CHEMICAL CONTAMINANTS; HEALTH INDICATORS;
HUDSON RIVER; BAY; FISH; PATTERNS
AB Contaminant bioaccumulation dynamics was examined in young-of-the-year (YOY) bluefish subpopulations (Pomatomus saltatrix) in the New York Bight ecosystem, and the results were used to assess (i) effects of habitat quality in terms of levels of PCBs and pesticides on bluefish condition and (ii) fidelity of YOY bluefish to different subestuaries that served as the nurseries subsequent to recruitment during their first summer. Total PCBs and p,p'=-DDE body burdens increased with fish length, but concentrations generally increased only poorly to moderately, which suggested steady-state contaminant uptake commensurate with aggressive feeding and dilution related to rapid growth characteristic of YOY bluefish within a subestuary. High condition factors paired with elevated contamination levels in bluefish from the Lower Hudson River, as compared with bluefish from Newark Bay with poor condition factors paired with elevated contamination levels, suggested that PCBs and pesticides alone may not determine condition in these fish. We found dissimilar patterns of prominent PCB congeners in bluefish from adjacent subestuaries (e.g., Newark Bay and Lower Hudson River) suggesting separate contaminant sources. Total PCB normalized fingerprints of PCB congeners permitted statistical discrimination among YOY bluefish specimens from various estuaries with a potential to differentiate subpopulations on scales to less than 20 km. This unexpected fidelity to nursery estuaries may have implications for the management strategies.
C1 [Deshpande, Ashok D.; Dockum, Bruce W.; Draxler, Andrew F. J.] NOAA, Sandy Hook Lab, Natl Marine Fisheries Serv, 74 Magruder Rd, Highlands, NJ 07732 USA.
RP Deshpande, AD (reprint author), NOAA, Sandy Hook Lab, Natl Marine Fisheries Serv, 74 Magruder Rd, Highlands, NJ 07732 USA.
EM ashok.deshpande@noaa.gov
NR 47
TC 1
Z9 1
U1 3
U2 4
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0706-652X
EI 1205-7533
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD JAN
PY 2016
VL 73
IS 1
BP 35
EP 52
DI 10.1139/cjfas-2015-0369
PG 18
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA DD6QK
UT WOS:000370048500004
ER
PT J
AU Cornwell, E
Molotch, NP
McPhee, J
AF Cornwell, E.
Molotch, N. P.
McPhee, J.
TI Spatio-temporal variability of snow water equivalent in the
extra-tropical Andes Cordillera from distributed energy balance modeling
and remotely sensed snow cover
SO HYDROLOGY AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID LAND-SURFACE TEMPERATURE; MODIS LST DATA; AIR-TEMPERATURE;
SOUTH-AMERICA; CENTRAL CHILE; RUNOFF MODEL; PRECIPITATION; PRODUCTS;
VALIDATION; RESOLUTION
AB Seasonal snow cover is the primary water source for human use and ecosystems along the extratropical Andes Cordillera. Despite its importance, relatively little research has been devoted to understanding the properties, distribution and variability of this natural resource. This research provides high-resolution (500 m), daily distributed estimates of end-of-winter and spring snow water equivalent over a 152 000 km(2) domain that includes the mountainous reaches of central Chile and Argentina. Remotely sensed fractional snow-covered area and other relevant forcings are combined with extrapolated data from meteorological stations and a simplified physically based energy balance model in order to obtain melt-season melt fluxes that are then aggregated to estimate the end-of-winter (or peak) snow water equivalent (SWE). Peak SWE estimates show an overall coefficient of determination R-2 of 0.68 and RMSE of 274 mm compared to observations at 12 automatic snow water equivalent sensors distributed across the model domain, with R-2 values between 0.32 and 0.88. Regional estimates of peak SWE accumulation show differential patterns strongly modulated by elevation, latitude and position relative to the continental divide. The spatial distribution of peak SWE shows that the 4000-5000 a.s.l. elevation band is significant for snow accumulation, despite having a smaller surface area than the 3000-4000 a.s.l. band. On average, maximum snow accumulation is observed in early September in the western Andes, and in early October on the eastern side of the continental divide. The results presented here have the potential of informing applications such as seasonal forecast model assessment and improvement, regional climate model validation, as well as evaluation of observational networks and water resource infrastructure development.
C1 [Cornwell, E.; McPhee, J.] Univ Chile, Fac Ciencias Fis & Matemat, Adv Min Technol Ctr, Santiago, Chile.
[Molotch, N. P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, N. P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Molotch, N. P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[McPhee, J.] Univ Chile, Fac Ciencias Fis & Matemat, Dept Ingn Civil, Santiago, Chile.
RP McPhee, J (reprint author), Univ Chile, Fac Ciencias Fis & Matemat, Adv Min Technol Ctr, Santiago, Chile.; McPhee, J (reprint author), Univ Chile, Fac Ciencias Fis & Matemat, Dept Ingn Civil, Santiago, Chile.
EM jmcphee@u.uchile.cl
RI McPhee, James/F-3402-2011; Molotch, Noah/C-8576-2009
OI McPhee, James/0000-0002-7547-0926;
FU CONICYT [FONDECYT 1121184, SER-03, FONDEF CA13I10277, CHILE-USA2013]
FX This research was conducted with support from CONICYT, under grants
FONDECYT 1121184, SER-03, FONDEF CA13I10277 and CHILE-USA2013. The
authors wish to thank everybody involved in field data collection,
including brothers Santiago and Gonzalo Montserrat, Mauricio Cartes,
Alvaro Ayala, and many others. Gonzalo Cortes provided insightful
comments to working drafts of this paper.
NR 67
TC 5
Z9 5
U1 5
U2 17
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1027-5606
EI 1607-7938
J9 HYDROL EARTH SYST SC
JI Hydrol. Earth Syst. Sci.
PY 2016
VL 20
IS 1
BP 411
EP 430
DI 10.5194/hess-20-411-2016
PG 20
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA DD1GD
UT WOS:000369668400024
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
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Besson, DZ
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CA IceCube Collaboration
IceCube Collaboration
Pierre Auger Collaboration
Pierre Auger Collaboration
Telescope Array Collaboration
TI Search for correlations between the arrival directions of IceCube
neutrino events and ultrahigh-energy cosmic rays detected by the Pierre
Auger Observatory and the Telescope Array
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE neutrino experiments; ultra high energy cosmic rays; cosmic ray
experiments; neutrino astronomy
ID GALACTIC MAGNETIC-FIELD; SURFACE DETECTOR; SPECTRUM; DEFLECTIONS;
PERFORMANCE
AB This paper presents the results of different searches for correlations between very high-energy neutrino candidates detected by IceCube and the highest-energy cosmic rays measured by the Pierre Auger Observatory and the Telescope Array. We first consider samples of cascade neutrino events and of high-energy neutrino-induced muon tracks, which provided evidence for a neutrino flux of astrophysical origin, and study their cross-correlation with the ultrahigh-energy cosmic ray (UHECR) samples as a function of angular separation. We also study their possible directional correlations using a likelihood method stacking the neutrino arrival directions and adopting different assumptions on the size of the UHECR magnetic deflections. Finally, we perform another likelihood analysis stacking the UHECR directions and using a sample of through-going muon tracks optimized for neutrino point-source searches with sub-degree angular resolution. No indications of correlations at discovery level are obtained for any of the searches performed. The smallest of the p-values comes from the search for correlation between UHECRs with IceCube high-energy cascades, a result that should continue to be monitored.
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[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
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[Adams, J.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.; Silva, A. H. Cruz] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Hansen, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
[Boerner, M.; Fuchs, T.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.; Neer, G.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Weaver, Ch.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C-C.; Koepke, L.; Kroll, G.; Krueckl, G.; Sander, H-G.; Sandroos, J.; Schatto, K.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Abraham, K.; Bernhard, A.; Coenders, S.; Gross, A.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, D-85748 Garching, Germany.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Kurahashi, N.; Richman, M.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; In, S.; Jeong, M.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Luenemann, J.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de Los Heros, C. Perez; Stroem, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Becker, K-H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H-P.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, 7-3-1 Hongo, Tokyo 113, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Allekotte, I.; Asorey, H.; Bertou, X.; Golup, G.; Gomez Berisso, M.; Harari, D.; Mollerachl, S.; Naranjo, I.; Roulet, E.; Taborda, O. A.] CNEA UNCuyo CONICET, Ctr Atom Bariloche, San Carlos De Bariloche, Rio Negro, Argentina.
[Allekotte, I.; Almela, A.; Asorey, H.; Bertou, X.; Golup, G.; Gomez Berisso, M.; Harari, D.; Mollerachl, S.; Naranjo, I.; Roulet, E.; Taborda, O. A.] CNEA UNCuyo CONICET, Inst Balseiro, San Carlos De Bariloche, Rio Negro, Argentina.
[Pallotta, J.; Quell, E. J.; Ristori, P.] CITEDEF, Ctr Invest Laseres & Aplicaciones, San Carlos De Bariloche, Rio Negro, Argentina.
[Dova, M. T.; Hansen, P.; Jarne, C.; Mariazzi, A. G.; Pallotta, J.; Quell, E. J.; Ristori, P.; Wahlberg, H.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.
[Dasso, S.; Meza, J. J. Masias; Piegaia, R.; Pieroni, P.] Univ Buenos Aires, Dept Fis, FCEyN, RA-1053 Buenos Aires, DF, Argentina.
[Dova, M. T.; Hansen, P.; Jarne, C.; Mariazzi, A. G.; Wahlberg, H.] Univ Nacl La Plata, IFLP, RA-1900 La Plata, Buenos Aires, Argentina.
[Dasso, S.; Rovero, A. C.; Salazar, H.; Supanitsky, A. D.] CONICET UBA, IAFE, Buenos Aires, DF, Argentina.
[Freire, M. M.; Micheletti, M. I.] UNR, CONICET, Inst Fis Rosario IFIR, Rosario, Santa Fe, Argentina.
[Freire, M. M.; Micheletti, M. I.] UNR, Fac Ciencias Bioquim & Farmaceut, Rosario, Santa Fe, Argentina.
[Garcia, B.] UNSAM, CONICET, CNEA, Inst Tecnol Detecc & Astroparticulas, Buenos Aires, DF, Argentina.
[Garcia, B.] Univ Tecnol Nacl, Fac Reg Mendoza, CONICET, CNEA, Mendoza, Argentina.
[Almela, A.; Andrada, B.; Botti, A. M.; Etchegoyen, A.; Figueira, J. M.; Filevich, A.; Fuster, A.; Gallo, F.; Gonzalez, N.; Hampel, M. R.; Josebachuili, M.; Lucero, A.; Melo, D.; Platino, M.; Ravignani, D.; Sanchez, F.; Suarez, F.; Tapia, A.; Videla, M.; Wainberg, O.; Wundheiler, B.] UNSAM, CONICET, Inst Tecnol Detecc & Astroparticulas,CNEA, Ctr Atom Constituyentes,Comis Nacl Engergia Atom, Buenos Aires, DF, Argentina.
[Avila, G.; Contreras, F.; Gomez Vitale, P. F.; Kleinfeller, J.; Rodriguez Rojo, J.; Salazar, H.; Sato, R.; Scarso, C.; Squartini, R.] Observ Pierre Auger, Mendoza, Argentina.
[Avila, G.; Gomez Vitale, P. F.] Comis Nacl Energia Atom, RA-1429 Buenos Aires, DF, Argentina.
[Almela, A.; Etchegoyen, A.; Fuster, A.; Gallo, F.; Suarez, F.; Wainberg, O.] Univ Tecnol Nacl, Fac Reg Buenos Aires, Buenos Aires, DF, Argentina.
[Bellido, J. A.; Blaess, S. G.; Clay, R. W.; Cooper, M. J.; Dawson, B. R.; Grubb, T. D.; Harrison, T. A.; Hill, G. C.; Malacari, M.; Nguyen, P. H.; Saffil, S. J.; Sorokin, J.; van Bodegom, P.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Maurizio, D.; Shellard, R. C.] CBPF, Rio De Janeiro, Brazil.
[Todero Peixoto, C. J.] Univ Sao Paulo, Escola Engn Lorena, BR-05508 Sao Paulo, Brazil.
[de Souza, V.; dos Anjos, R. C.; Prado, R. R.] Univ Sao Paulo, Inst Fis Sao Carlos, Sao Carlos, SP, Brazil.
[Albuquerque, I. F. M.; Gouffon, P.; Santos, E. M.] Univ Sao Paulo, Inst Fis, CP 20516, BR-01498 Sao Paulo, Brazil.
[Chinellato, J. A.; Daniel, B.; Castro, M. L. Diaz; Dobrigkeit, C.; Escobar, C. O.; Fauth, A. C.; Kemp, E.; Muller, M. A.; Selmi-Dei, D. Pakk; Santos, E.; Theodoro, V. M.] Univ Estadual Campinas UNICAMP, Campinas, SP, Brazil.
[Guedes, G. P.] Univ Estadual Feira de Santana, Feira de Santana, BA, Brazil.
[Pepe, I. M.] Univ Fed Bahia, BR-41170290 Salvador, BA, Brazil.
[Muller, M. A.] Univ Fed Pelotas, Pelotas, Brazil.
[Leigui de Oliveira, M. A.; Moura, C. A.] Univ Fed Abc, Santo Andre, Brazil.
[Bonifazi, C.; de Mello Neto, J. R. T.; Giaccari, U.; Mello, V. B. B.; Torres Machado, D.; Vasquez, R.] Univ Fed Rio de Janeiro, Inst Fis, Rio de Janeiro, Brazil.
[de Almeida, R. M.; de Oliveira, J.] Univ Fed Fluminense, BR-24220000 Niteroi, RJ, Brazil.
[Asorey, H.; Nunez, L. A.; Pena-Rodriguez, J.; Sanabria Gomez, J. D.; Sarmiento-Cano, C.; Duran, M. Suarez] Univ Ind Santander, Santander, Spain.
[Blazek, J.; Bohacova, M.; Chudoba, J.; Ebr, J.; Mandat, D.; Necesal, P.; Palatka, M.; Pech, M.; Prouza, M.; Ridky, J.; Schovanek, P.; Travnicek, P.; Vicha, J.] Acad Sci Czech Republic, Inst Phys FZU, Prague, Czech Republic.
[Horvath, P.; Hrabovsksy, M.; Nozka, H.] Palacky Univ, RCPTM, Olomouc, Czech Republic.
[Nosek, D.; Novotny, V.] Univ Prague, Inst Particle & Nucl Phys, Prague, Czech Republic.
[Deligny, O.; Lhenry-Yvon, I.; Suomijarvi, T.; Zong, Z.] Univ Paris 11, CNRS, IN2P3, IPNO, Orsay, France.
[Cordier, A.; Garcia-Gamez, D.] Univ Paris 11, CNRS, IN2P3, LAL, Orsay, France.
[Al Samarai, I.; Aublin, J.; Billoir, P.; Blanco, M.; Caccianiga, L.; Ghia, P. L.; Letessier-Selvon, A.; Settimo, M.] Univ Paris 06, LPNHE, F-75252 Paris 05, France.
[Al Samarai, I.; Aublin, J.; Billoir, P.; Blanco, M.; Caccianiga, L.; Ghia, P. L.; Letessier-Selvon, A.; Settimo, M.] Univ Paris 07, CNRS, IN2P3, F-75221 Paris 05, France.
[Berat, C.; Lebrun, D.; Montanet, F.; Stutz, A.] Univ Grenoble Alpes, CNRS, IN2P3, LPSC, St Martin Dheres, France.
[Dallier, R.] Stn Radioastron Nancay, Nancay, France.
[Dallier, R.; Gate, F.; Lautridou, P.; Marin, V.; Ravel, O.; Revenu, B.] Univ Nantes, CNRS, IN2P3, Ecole Mines Nantes,SUBATECH, F-44035 Nantes, France.
[Becker, K. H.; Jandt, I.; Kaeaepae, A.; Kampert, K. H.; Krohm, N.; Mathys, S.; Neuser, J.; Niemietz, L.; Papenbreer, P.; Querchfeld, S.; Rautenberg, J.; Sarkar, B.; Schauer, M.; Winchen, T.; Wittkowski, D.] Berg Univ Wuppertal, Fachbereich Phys C, Wuppertal, Germany.
[Baus, C.; Bluemer, H.; Herve, A. E.; Kambeitz, O.; Katkov, I.; Link, K.] Karlsruhe Inst Technol, IEKP, D-76021 Karlsruhe, Germany.
[Bluemer, H.; Bridgeman, A.; Daumiller, K.; Debatin, J.; Engel, R.; Hasankiadeh, Q.; Haungs, A.; Heck, D.; Holt, E.; Huege, T.; Keilhauer, B.; Klages, H. O.; Awad, A. Kuotb; Mathes, H. J.; Mueller, S.; Pierog, T.; Rogozin, D.; Roth, M.; Schieler, H.; Schmidt, D.; Schroeder, F. G.; Schulz, A.; Smida, R.; Tomankova, L.; Ulrich, R.; Unger, M.; Veberic, D.; Weindl, A.] Karlsruhe Inst Technol, IKP, D-76021 Karlsruhe, Germany.
[Gemmeke, H.; Kleifges, M.; Kunka, N.; Menshikov, A.; Weber, M.; Zimmermann, B.] Karlsruhe Inst Technol, IPE, D-76021 Karlsruhe, Germany.
[Bretz, T.; Briechle, F. L.; Erdmann, M.; Glaser, C.; Hebbeker, T.; Krause, R.; Kuempel, D.; Lauscher, M.; Middendorf, L.; Mueller, G.; Niggemann, T.; Peters, C.; Plum, M.; Reinert, D.; Schumacher, J.; Stephan, M.; Urban, M.; Walz, D.; Weidenhaupt, K.] Rhein Westfal TH Aachen, Inst Phys 3A, Aachen, Germany.
[Batista, R. Alves; Dundovic, A.; Sigl, G.] Univ Hamburg, Inst Theoret Phys 2, Hamburg, Germany.
[Aab, A.; Buchholz, P.; Erfani, M.; Heimann, P.; Niechcio, M.; Ochilo, L.; Risse, M.; Sonntag, S.; Tepe, A.; Yushkov, A.; Ziolkowski, M.] Univ Siegen, Fachbereich Phys Expt Teilchenphys 7, D-57068 Siegen, Germany.
[Segreto, A.] Ist Nazl Fis Nucl, Ist Astrofis Spaziale & Fis Cosm Palermo, Palermo, Italy.
[Boncioli, D.; Grillo, A. F.] INFN Lab Gran Sasso, Gran Sasso, Italy.
[Buscemi, M.; Caruso, R.; Insolia, A.; Pirronello, V.; Segreto, A.; Zuccarello, F.] Ist Nazl Fis Nucl, Sez Catania, Catania, Italy.
[Di Matteo, A.; Petrera, S.; Rizi, V.] Ist Nazl Fis Nucl, Sez Aquila, Laquila, Italy.
[Bleve, C.; Cataldi, G.; Coluccia, M. R.; D'Amico, S.; De Mitri, I.; Marsella, G.; Martello, D.; Perrone, L.; Scherini, V.; Strafella, F.] Ist Nazl Fis Nucl, Sez Lecce, Lecce, Italy.
[Caccianiga, B.; Giammarchi, M.; Mallamaci, M.; Miramonti, L.] Ist Nazl Fis Nucl, Sez Milano, Milan, Italy.
[Ambrosio, M.; Aramo, C.; Colalillo, R.; Guarino, F.; Valore, L.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Candusso, M.; Di Giulio, C.; Matthiae, G.; Salina, G.; Verzi, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Aglietta, M.; Bertaina, M. E.; Castellina, A.; Cester, R.; Chiavassa, A.; Collica, L.; Gorgi, A.; Latronico, L.; Morello, C.; Tonachini, A.] Ist Nazl Fis Nucl, Sez Torino, Turin, Italy.
[Aglietta, M.; Castellina, A.; Gorgi, A.; Morello, C.] Osservatorio Astrofis Torino INAF, Turin, Italy.
[Bertaina, M. E.; Cester, R.; Chiavassa, A.; Tonachini, A.] Univ Turin, Dipartimento Fis, I-10124 Turin, Italy.
[D'Amico, S.] Univ Salento, Dipartimento Ingn, Lecce, Italy.
[Bleve, C.; Coluccia, M. R.; De Mitri, I.; Marsella, G.; Martello, D.; Perrone, L.; Scherini, V.; Strafella, F.] Univ Salento, Dipartimento Matemat & Fis E De Giorgi, Lecce, Italy.
[Caruso, R.; Di Matteo, A.; Petrera, S.; Rizi, V.] Univ Aquila, Dipartimento Chim & Fis, I-67100 Laquila, Italy.
[Buscemi, M.; Insolia, A.; Pirronello, V.; Zuccarello, F.] Univ Catania, Dipartimento Fis & Astron, I-95124 Catania, Italy.
[Mallamaci, M.; Miramonti, L.] Univ Milan, Dipartimento Fis, I-20122 Milan, Italy.
[Colalillo, R.; Guarino, F.; Valore, L.] Univ Naples Federico II, Dipartimento Fis, Naples, Italy.
[Di Giulio, C.; Matthiae, G.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Lopez, R.; Bravo, O. Martinez; Parra, A.; Varela, E.] BUAP, Puebla, Mexico.
[Martinez, H.; Zepeda, A.] CINVESTAV, Ctr Invest & Estudios Avanzados IPN, Mexico City, DF, Mexico.
[Pelayo, R.] UPIITA IPN, Mexico City, DF, Mexico.
[Caballero-Mora, K. S.] Univ Autonoma Chiapas, Tuxtla Gutierrez, Mexico.
[Chavez, A. G.; Villasenor, L.] Univ Michoacana, Morelia, Michoacan, Mexico.
[Castillo, J. Alvarez; D'Olivo, J. C.; Medina-Tanco, G.; Nellen, L.; Galicia, J. F. Valdes; Vargas Cardenas, B.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico.
[Aminaei, A.; Buitink, S.; de Jong, S. J.; De Mauro, G.; Falcke, H.; Hoerandel, J. R.; Jansen, S.; Nelles, A.; Schulz, J.; Timmermans, C.; van Aar, G.; van Vliet, A.; Wykes, S.] Radboud Univ Nijmegen, IMAPP, NL-6525 ED Nijmegen, Netherlands.
[Docters, W.; Messina, S.; Scholtene, .; van den Berg, A. M.] Univ Groningen, KVI Ctr Adv Radiat Technol, NL-9700 AB Groningen, Netherlands.
[de Jong, S. J.; Falcke, H.; Hoerandel, J. R.; Jansen, S.; Nelles, A.; Timmermans, C.] NIKHEF, Amsterdam, Netherlands.
[Falcke, H.] Stichting Astron Onderzoek Nederland ASTRON, Dwingeloo, Netherlands.
[Borodai, N.; Homola, P.; Pekala, J.; Porowski, C.; Privitera, P.; Stasielak, J.; Wilczynski, H.] Inst Phys Nucl PAN, Krakow, Poland.
[Giller, M.; Glas, D.; Smialkowski, A.; Szadkowski, Z.] Univ Lodz, PL-90131 Lodz, Poland.
[Abreu, P.; Andringa, S.; Assis, P.; Blanco, A.; Cazon, L.; Conceicao, R.; Diogo, F.; Espadanal, J.; Lopes, L.; Pimenta, M.; Sarmento, R.; Tome, B.] Univ Lisbon, Lab Instrumentacao Fis Expt Particulas LIP, Lisbon, Portugal.
[Abreu, P.; Andringa, S.; Assis, P.; Blanco, A.; Cazon, L.; Conceicao, R.; Diogo, F.; Espadanal, J.; Lopes, L.; Pimenta, M.; Sarmento, R.; Tome, B.] Univ Lisbon, IST, Lisbon, Portugal.
[Brancus, I.; Gherghel-Lascu, A.; Mitrica, B.; Niculescu-Oglinzanu, M.; Saftoiu, A.; Stanca, D.; Toma, G.] Horia Hulubei Natl Inst Phys & Nucl Engn, Bucharest 077125, Romania.
[Caramete, L.; Isar, P. G.] Inst Space Sci, Bucharest, Romania.
[Arsene, N.; Sima, O.] Univ Bucharest, Dept Phys, Bucharest, Romania.
[Badescu, A. M.; Fratu, O.] Univ Politehn Bucuresti, Bucharest, Romania.
[Filipi, A.; Zavrtanik, D.; Zavrtanik, M.] Jozef Stefan Inst, Expt Particle Phys Dept, Ljubljana, Slovenia.
[Filipi, A.; Mezek, G. Kukec; Saleh, A.; Stanic, S.; Trini, M.; Vorobiov, S.; Yang, L.; Zavrtanik, D.; Zavrtanik, M.] Univ Nova Gorica, Lab Astroparticle Phys, Nova Gorica, Slovenia.
[Arqueros, F.; Garcia-Pinto, D.; Minaya, I. A.; Rosado, J.; Vazquez, J. R.] Univ Complutense Madrid, E-28040 Madrid, Spain.
[del Peral, L.; Pacheco, N.; Rodriguez-Frias, M. D.] Univ Alcala de Henares, E-28871 Alcala De Henares, Spain.
[Bueno, A.; Maris, I. C.; Molina-Bueno, L.; Navas, S.; Sanchez-Lucas, P.] Univ Granada, E-18071 Granada, Spain.
[Alvarez-Muniz, J.; Lopez Casado, A.; Parente, G.; Rodrigues de Carvalho, W.; Elipe, G. Torralba; Valino, I.; Vazquez, R. A.; Zas, E.] Univ Santiago Compostela, Santiago De Compostela, Spain.
[Covault, C. E.; Ferguson, A. P.; LaHurd, D.; Quinn, S.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Johnsen, J. A.; Mayotte, E.; Medina, C.; Sarazin, F.; Wiencke, L.] Colorado Sch Mines, Golden, CO 80401 USA.
[Anchordoqui, L.; Pau, T.] CUNY, Lehman Coll, Dept Phys & Astron, New York, NY USA.
[Ahn, E. J.; Escobar, C. O.; Fazzini, N.; Glass, H.; Hojvat, C.; Kasper, P.; Lebrun, P.; Mantsch, P.; Mazur, P. O.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Matthews, J.; Shadkam, A.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Diaz, J. C. Chirinos; Dhital, N.; Fick, B.; Kieckhafer, R. M.; Nitz, D.; Yapici, T.] Michigan Technol Univ, Houghton, MI 49931 USA.
[Awal, N.; Farrar, G.; Unger, M.] New York Univ, New York, NY USA.
[Pau, T.; Swain, J.] Northeastern Univ, Boston, MA USA.
[Allison, P.; Beatty, J. J.; Gordon, J.; Griffith, N.; Stapleton, J.; Sutherland, M. S.] Ohio State Univ, Columbus, OH 43210 USA.
[Coleman, A.; Coutu, S.; Mostafa, M.; Oikonomou, F.; Phuntsok, J.; Greus, F. Salesa; Sommers, P.] Penn State Univ, University Pk, PA 16802 USA.
[Fang, K.; Fujii, T.; Hollon, N.; Olinto, A.] Univ Chicago, Chicago, IL 60637 USA.
[Gorham, P.; Schoorlemmer, H.; Varner, G.] Univ Hawaii, Honolulu, HI 96822 USA.
[Lauer, R.; Matthews, J. A. J.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Watson, A. A.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England.
[Biermann, P. L.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Scholtene, .] Vrije Univ Brussel, Brussels, Belgium.
[dos Anjos, R. C.] Univ Fed Parana, Palotina, PR, Brazil.
[Abbasi, R. U.; Abu-Zayyad, T.; Allen, M.; Barcikowski, E.; Belz, J. W.; Bergman, D. R.; Blake, S. A.; Cady, R.; Hanlon, W.; Ivanov, D.; Jui, C. C. H.; Kim, J. H.; Lan, J.; Lundquist, J. P.; Matthews, J. N.; Myers, I.; Rodriguez, D. C.; Shah, P. D.; Smith, J. D.; Sokolsky, P.; Springer, R. W.; Stokes, B. T.; Stratton, S. R.; Stroman, T. A.; Thomas, S. B.; Thomson, G. B.; Vasiloff, G.; Wong, T.; Zollinger, R.; Zundel, Z.] Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT USA.
[Abe, M.; Inoue, N.; Kawana, S.; Nagasawa, K.; Suzawa, T.] Saitama Univ, Grad Sch Sci & Engn, Saitama 3388570, Japan.
[Azuma, R.; Ishimori, R.; Kakimoto, F.; Kitamura, S.; Kitamura, Y.; Ogura, J.; Tokuno, H.; Tsunesada, Y.; Tsutsumi, K.] Tokyo Inst Technol, Grad Sch Sci & Engn, Tokyo 152, Japan.
[Chae, M. J.; Lim, S. I.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul, South Korea.
[Chae, M. J.; Lim, S. I.; Yang, J.] Ewha Womans Univ, Inst Early Univ, Seoul, South Korea.
[Cheon, B. G.; Kim, H. B.; Shins, B. K.] Hanyang Univ, Dept Phys, Seoul 133791, South Korea.
[Cheon, B. G.; Kim, H. B.; Shins, B. K.] Hanyang Univ, Res Inst Nat Sci, Seoul 133791, South Korea.
[Chiba, J.; Takamura, M.; Yashiro, K.] Tokyo Univ Sci, Dept Phys, Noda, Chiba 278, Japan.
[Chikawa, M.; Nozato, A.] Kinki Univ, Dept Phys, Higashiosaka, Osaka 577, Japan.
[Cho, W. R.; Kwon, Y. J.] Yonsei Univ, Dept Phys, Seoul 120749, South Korea.
[Fujii, T.; Fukushima, M.; Ikeda, D.; Kawata, K.; Kido, E.; Nonaka, T.; Ohnishi, M.; Ohoka, H.; Oki, K.; Sagawa, H.; Shibata, T.; Shimodaira, H.; Shin, H. S.; Takeda, M.; Takeishi, R.; Takita, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan.
[Fukushima, M.; Martens, K.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba, Japan.
[Gotoll, T.; Hayashi, Y.; Kawakami, S.; Matsuyama, T.; Minamino, M.; Ogioll, S.; Sakurai, N.; Tanaka, H.; Yamane, R.; Yoneda, Y.] Osaka City Univ, Grad Sch Sci, Osaka 558, Japan.
[Hayashida, N.; Hibino, K.; Tameda, Y.; Udo, S.] Kanagawa Univ, Fac Engn, Yokohama, Kanagawa, Japan.
[Honda, K.; Ishii, T.; Machida, K.; Mukai, Y.; Shibata, F.] Yamanashi Univ, Interdisciplinary Grad Sch Med & Engn, Kofu, Yamanashi 400, Japan.
[Ito, H.; Nagataki, S.] RIKEN, Astrophys Big Bang Lab, Wako, Saitama, Japan.
[Kadota, K.] Tokyo City Univ, Dept Phys, Setagaya Ku, Tokyo, Japan.
[Kalashev, O.; Kuzmin, V.; Pshirkov, M. S.; Rubtsov, G.; Tinyakov, P.; Tkachev, I.; Troitsky, S.] Russian Acad Sci, Inst Nucl Res, Moscow 117312, Russia.
[Kasahara, K.; Ozawa, S.] Waseda Univ, Adv Res Inst Sci & Engn, Shinjuku Ku, Tokyo, Japan.
[Kawail, H.; Yoshida, S.] Chiba Univ, Dept Phys, 1-33 Yayoi Cho, Chiba 260, Japan.
[Kim, J. H.; Ryu, D.] UNIST Gil, Ulsan Natl Inst Sci & Technol, Sch Nat Sci, Dept Phys, Ulsan, South Korea.
[Matsuda, T.; Tanaka, M.; Yamaoka, H.] KEK, Inst Particle & Nucl Studies, Tsukuba, Ibaraki, Japan.
[Nakamura, T.] Kochi Univ, Fac Sci, Kochi 780, Japan.
[Okuda, T.] Ritsumeikan Univ, Dept Phys Sci, Kusatsu, Shiga, Japan.
[Ono, M.] Kyushu Univ, Dept Phys, Fukuoka 812, Japan.
[Oshima, A.] Chubu Univ, Engn Sci Lab, Kasugai, Aichi 487, Japan.
[Park, I. H.] Sungkyunkwan Univ, Dept Phys, Suwon, South Korea.
[Pshirkov, M. S.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Scott, L. M.; Stratton, S. R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA.
[Taketa, A.; Yamazaki, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, 7-3-1 Hongo, Tokyo 113, Japan.
[Tanaka, K.] Hirosaki City Univ, Grad Sch Informat Sci, Hiroshima, Japan.
[Tinyakov, P.; Urban, F.] Univ Libre Bruxelles, Serv Phys Theor, Brussels, Belgium.
[Tomida, T.] Shinshu Univ, Dept Comp Sci & Engn, Nagano, Japan.
[Uchihori, Y.] Natl Inst Radiol Sci, Chiba 260, Japan.
[Yoshii, H.] Ehime Univ, Dept Phys, Matsuyama, Ehime, Japan.
RP Aartsen, MG (reprint author), Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
RI Alvarez-Muniz, Jaime/H-1857-2015; Gouffon, Philippe/I-4549-2012; de
Almeida, Rogerio/L-4584-2016; Fauth, Anderson/F-9570-2012; Maruyama,
Reina/A-1064-2013; KIM, JIHYUN/F-2353-2011; Abreu, Pedro/L-2220-2014;
Assis, Pedro/D-9062-2013; Navas, Sergio/N-4649-2014; Arqueros,
Fernando/K-9460-2014; Cazon, Lorenzo/G-6921-2014; Badescu,
Alina/B-6087-2012; Tome, Bernardo/J-4410-2013; Tjus, Julia/G-8145-2012;
Rubtsov, Grigory/K-8475-2012; Rosado, Jaime/K-9109-2014; zas,
enrique/I-5556-2015; Chinellato, Jose Augusto/I-7972-2012; Pshirkov,
Maxim/B-5324-2014; Caramete, Laurentiu/C-2328-2011; Chinellato, Carola
Dobrigkeit /F-2540-2011; Moura Santos, Edivaldo/K-5313-2016; Horvath,
Pavel/G-6334-2014; Sarkar, Subir/G-5978-2011; Wiebusch,
Christopher/G-6490-2012; Koskinen, David/G-3236-2014; De Mitri,
Ivan/C-1728-2017; Mitrica, Bogdan/D-5201-2009; Alves Batista,
Rafael/K-6642-2012; Nosek, Dalibor/F-1129-2017; Troitsky,
Sergey/C-1377-2014; Ridky, Jan/H-6184-2014; Conceicao,
Ruben/L-2971-2014; Bueno, Antonio/F-3875-2015; Beatty,
James/D-9310-2011; Sao Carlos Institute of Physics,
IFSC/USP/M-2664-2016; de Mello Neto, Joao/C-5822-2013; de souza,
Vitor/D-1381-2012; Guarino, Fausto/I-3166-2012; Zuccarello,
Francesca/R-1834-2016; Colalillo, Roberta/R-5088-2016; Buscemi,
Mario/R-5071-2016; Valino, Ines/J-8324-2012; Kalashev, Oleg/R-9476-2016;
OI Alvarez-Muniz, Jaime/0000-0002-2367-0803; Gouffon,
Philippe/0000-0001-7511-4115; de Almeida, Rogerio/0000-0003-3104-2724;
Fauth, Anderson/0000-0001-7239-0288; Maruyama,
Reina/0000-0003-2794-512X; KIM, JIHYUN/0000-0002-8814-031X; Abreu,
Pedro/0000-0002-9973-7314; Assis, Pedro/0000-0001-7765-3606; Navas,
Sergio/0000-0003-1688-5758; Arqueros, Fernando/0000-0002-4930-9282;
Cazon, Lorenzo/0000-0001-6748-8395; Tome, Bernardo/0000-0002-7564-8392;
Rubtsov, Grigory/0000-0002-6106-2673; Rosado, Jaime/0000-0001-8208-9480;
zas, enrique/0000-0002-4430-8117; Chinellato, Jose
Augusto/0000-0002-3240-6270; Pshirkov, Maxim/0000-0002-5746-2017;
Chinellato, Carola Dobrigkeit /0000-0002-1236-0789; Moura Santos,
Edivaldo/0000-0002-2818-8813; Rizi, Vincenzo/0000-0002-5277-6527; Garcia
Pinto, Diego/0000-0003-1348-6735; Perez de los Heros,
Carlos/0000-0002-2084-5866; Horvath, Pavel/0000-0002-6710-5339; Sarkar,
Subir/0000-0002-3542-858X; Wiebusch, Christopher/0000-0002-6418-3008;
Koskinen, David/0000-0002-0514-5917; De Mitri, Ivan/0000-0002-8665-1730;
Alves Batista, Rafael/0000-0003-2656-064X; Nosek,
Dalibor/0000-0001-6219-200X; Troitsky, Sergey/0000-0001-6917-6600;
Ridky, Jan/0000-0001-6697-1393; Conceicao, Ruben/0000-0003-4945-5340;
Bueno, Antonio/0000-0002-7439-4247; Beatty, James/0000-0003-0481-4952;
de Mello Neto, Joao/0000-0002-3234-6634; Guarino,
Fausto/0000-0003-1427-9885; Zuccarello, Francesca/0000-0003-1853-2550;
Colalillo, Roberta/0000-0002-4179-9352; Buscemi,
Mario/0000-0003-2123-5434; Valino, Ines/0000-0001-7823-0154; Kalashev,
Oleg/0000-0002-7982-1842; Arguelles Delgado, Carlos/0000-0003-4186-4182;
Del Peral, Luis/0000-0003-2580-5668; Novotny,
Vladimir/0000-0002-4319-4541; Strotjohann, Nora
Linn/0000-0002-4667-6730; Garcia, Beatriz/0000-0003-0919-2734
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Swedish Research Council,
Sweden; Swedish Polar Research Secretariat, Sweden; Swedish National
Infrastructure for Computing (SNIC), Sweden; Knut and Alice Wallenberg
Foundation, Sweden; German Ministry for Education and Research (BMBF),
Germany; Deutsche Forschungsgemeinschaft (DFG), Germany; Helmholtz
Alliance for Astroparticle Physics (HAP), Germany; Research Department
of Plasmas with Complex Interactions (Bochum), Germany; Fund for
Scientific Research (FNRS-FWO) (Belspo); FWO Odysseus programme
(Belspo); Flanders Institute to encourage scientific and technological
research in industry (IWT) (Belspo); Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Australian Research Council; Japan Society for Promotion of
Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland;
National Research Foundation of Korea (NRF); Danish National Research
Foundation, Denmark (DNRF); Natural Sciences and Engineering Research
Council of Canada, WestGrid and Compute/Calcul Canada; Comision Nacional
de Energia Atomica, Argentina; Agencia Nacional de Promocion Cientifica
y Tecnologica (ANPCyT), Argentina; Consejo Nacional de Investigaciones
Cientificas y Tecnicas (CONICET), Argentina; Gobierno de la Provincia de
Mendoza, Argentina; Municipalidad de Malargue, Argentina; NDM Holdings,
Argentina; Valle Las Lenas, Argentina; Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil; Financiadora de
Estudos e Projetos (FINEP), Brazil; Fundacao de Amparo a Pesquisa do
Estado de Rio de Janeiro (FAPERJ), Brazil; Sao Paulo Research Foundation
(FAPESP), Brazil [2010/07359-6, 1999/05404-3]; Ministerio de Ciencia e
Tecnologia (MCT), Brazil; Czech Science Foundation, Czech Republic
[14-17501S]; Centre de Calcul IN2P3/CNRS, France; Centre National de la
Recherche Scientifique (CNRS), France; Conseil Regional Ile-de-France,
France; Departement Physique Nucleaire et Corpusculaire, France
[PNC-IN2P3/CNRS]; Departement Sciences de l'Univers (SDU-INSU/CNRS),
France; Institut Lagrange de Paris (ILP) within the Investissements
d'Avenir Programme, France [LABEX ANR-10-LABX-63, ANR-11-IDEX-0004-02];
Bundesministerium fur Bildung und Forschung (BMBF), Germany;
Finanzministerium Baden-Wurttemberg, Germany; Helmholtz-Gemeinschaft
Deutscher Forschungszentren (HGF), Germany; Ministerium fur Wissenschaft
und Forschung, Germany; Nordrhein Westfalen, Germany; Ministerium fur
Wissenschaft, Germany; Forschung und Kunst, Germany; Baden-Wurttemberg,
Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Istituto
Nazionale di Astrofisica (INAF), Italy; Ministero dell'Istruzione,
Italy; dell'Universita e della Ricerca (MIUR), Italy; Gran Sasso Center
for Astroparticle Physics (CFA), Italy; CETEMPS Center of Excellence,
Italy; Ministero degli Affari Esteri (MAE), Italy; Consejo Nacional de
Ciencia y Tecnologia (CONACYT), Mexico; Ministerie van Onderwijs,
Netherlands; Cultuur en Wetenschap, Netherlands; Nederlandse Organisatie
voor Wetenschappelijk Onderzoek (NWO), Netherlands; Stichting voor
Fundamenteel Onderzoek der Materie (FOM), Netherlands; National Centre
for Research and Development, Poland [ERA-NET-ASPERA/01/11,
ERA-NET-ASPERA/02/11]; National Science Centre, Poland
[2013/08/M/ST9/00322, 2013/08/M/ST9/00728, HARMONIA 5 -
2013/10/M/ST9/00062]; Portuguese national funds, Portugal; FEDER funds
within Programa Operacional Factores de Competitividade through Fundacao
para a Ciencia e a Tecnologia (COMPETE), Portugal; Romanian Authority
for Scientific Research ANCS, Romania; CNDI-UEFISCDI partnership
projects, Romania [20/2012, 194/2012, 1/AS-PERA2/2012 ERA-NET,
PN-II-RU-PD-2011-3-0145-17, PN-II-RU-PD-2011-3-0062]; Minister of
National Education, Romania; Programme Space Technology and Advanced
Research (STAR), Romania; [83/2013]; Slovenian Research Agency,
Slovenia; Comunidad de Madrid, Spain; FEDER funds, Spain; Ministerio de
Educacion y Ciencia, Spain; Xunta de Galicia, Spain; European Community
7th Framework Program, Spain [FP7-PEOPLE-2012-IEF-328826]; Science and
Technology Facilities Council, United Kingdom, U.S.A.; Department of
Energy, U.S.A. [DE-AC02-07CH11359, DE-FR02-04ER41300, DE-FG02-99ER41107,
DE-SC0011689]; National Science Foundation, U.S.A. [0450696]; Grainger
Foundation, U.S.A.; NAFOSTED, Vietnam; Marie Curie-IRSES/EPLANET;
European Particle Physics Latin American Network; European Union 7th
Framework Program [PIRSES-2009-GA-246806, PIOF-GA-2013-624803]; UNESCO;
Japan Society for the Promotion of Science [21000002, 19104006];
Inter-University Research Program of the Institute for Cosmic Ray
Research; U.S. National Science Foundation [PHY-0307098, PHY-0601915,
PHY-0649681, PHY-0703893, PHY-0758342, PHY-0848320, PHY-1069280,
PHY-1069286, PHY-1404495, PHY-1404502]; National Research Foundation of
Korea [2007-0093860, R32-10130, 2012R1A1A2008381, 2013004883]; Russian
Academy of Sciences; RFBR [11-02-01528a, 13-02-01311a (INR)]; IISN
[4.4502.13]; Belgian Science Policy under IUAP (ULB) [VII/37 (ULB)];
State of Utah through its Economic Development Board; University of Utah
through the Office of the Vice President for Research; [MSMT-CR
LG13007]; [7AMB14AR005]
FX The IceCube Collaboration acknowledges the support from the following
agencies: U.S. National Science Foundation-Office of Polar Programs,
U.S. National Science Foundation Physics Division, University of
Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin
(GLOW) grid infrastructure at the University of Wisconsin Madison, the
Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy,
and National Energy Research Scientific Computing Center, the Louisiana
Optical Network Initiative (LONI) grid computing resources; Natural
Sciences and Engineering Research Council of Canada, WestGrid and
Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research
Secretariat, Swedish National Infrastructure for Computing (SNIC), and
Knut and Alice Wallenberg Foundation, Sweden; German Ministry for
Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG),
Helmholtz Alliance for Astroparticle Physics (HAP), Research Department
of Plasmas with Complex Interactions (Bochum), Germany; Fund for
Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders
Institute to encourage scientific and technological research in industry
(IWT), Belgian Federal Science Policy Office (Belspo); University of
Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research
Council; Japan Society for Promotion of Science (JSPS); the Swiss
National Science Foundation (SNSF), Switzerland; National Research
Foundation of Korea (NRF); Danish National Research Foundation, Denmark
(DNRF).; The successful installation, commissioning, and operation of
the Pierre Auger Observatory would not have been possible without the
strong commitment and effort from the technical and administrative staff
in Malargue. We are very grateful to the following agencies and
organizations for financial support: Comision Nacional de Energia
Atomica, Agencia Nacional de Promocion Cientifica y Tecnologica
(ANPCyT), Consejo Nacional de Investigaciones Cientificas y Tecnicas
(CONICET), Gobierno de la Provincia de Mendoza, Municipalidad de
Malargue, NDM Holdings and Valle Las Lenas, in gratitude for their
continuing cooperation over land access, Argentina; the Australian
Research Council; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico (CNPq), Financiadora de Estudos e Projetos (FINEP), Fundacao
de Amparo a Pesquisa do Estado de Rio de Janeiro (FAPERJ), Sao Paulo
Research Foundation (FAPESP) Grants No. 2010/07359-6 and No.
1999/05404-3, Ministerio de Ciencia e Tecnologia (MCT), Brazil; Grant
No. MSMT-CR LG13007, No. 7AMB14AR005, and the Czech Science Foundation
Grant No. 14-17501S, Czech Republic; Centre de Calcul IN2P3/CNRS, Centre
National de la Recherche Scientifique (CNRS), Conseil Regional
Ile-de-France, Departement Physique Nucleaire et Corpusculaire
(PNC-IN2P3/CNRS), Departement Sciences de l'Univers (SDU-INSU/CNRS),
Institut Lagrange de Paris (ILP) Grant No. LABEX ANR-10-LABX-63, within
the Investissements d'Avenir Programme Grant No. ANR-11-IDEX-0004-02,
France; Bundesministerium fur Bildung und Forschung (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Finanzministerium Baden-Wurttemberg,
Helmholtz Alliance for Astroparticle Physics (HAP),
Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF), Ministerium
fur Wissenschaft und Forschung, Nordrhein Westfalen, Ministerium fur
Wissenschaft, Forschung und Kunst, Baden-Wurttemberg, Germany; Istituto
Nazionale di Fisica Nucleare (INFN), Istituto Nazionale di Astrofisica
(INAF), Ministero dell'Istruzione, dell'Universita e della Ricerca
(MIUR), Gran Sasso Center for Astroparticle Physics (CFA), CETEMPS
Center of Excellence, Ministero degli Affari Esteri (MAE), Italy;
Consejo Nacional de Ciencia y Tecnologia (CONACYT), Mexico; Ministerie
van Onderwijs, Cultuur en Wetenschap, Nederlandse Organisatie voor
Wetenschappelijk Onderzoek (NWO), Stichting voor Fundamenteel Onderzoek
der Materie (FOM), Netherlands; National Centre for Research and
Development, Grants No. ERA-NET-ASPERA/01/11 and No.
ERA-NET-ASPERA/02/11, National Science Centre, Grants No.
2013/08/M/ST9/00322, No. 2013/08/M/ST9/00728 and No. HARMONIA 5 -
2013/10/M/ST9/00062, Poland; Portuguese national funds and FEDER funds
within Programa Operacional Factores de Competitividade through Fundacao
para a Ciencia e a Tecnologia (COMPETE), Portugal; Romanian Authority
for Scientific Research ANCS, CNDI-UEFISCDI partnership projects Grants
No. 20/2012 and No. 194/2012, Grants No. 1/AS-PERA2/2012 ERA-NET, No.
PN-II-RU-PD-2011-3-0145-17 and No. PN-II-RU-PD-2011-3-0062, the Minister
of National Education, Programme Space Technology and Advanced Research
(STAR), Grant No. 83/2013, Romania; Slovenian Research Agency, Slovenia;
Comunidad de Madrid, FEDER funds, Ministerio de Educacion y Ciencia,
Xunta de Galicia, European Community 7th Framework Program, Grant No.
FP7-PEOPLE-2012-IEF-328826, Spain; Science and Technology Facilities
Council, United Kingdom; Department of Energy, Contracts No.
DE-AC02-07CH11359, No. DE-FR02-04ER41300, No. DE-FG02-99ER41107 and No.
DE-SC0011689, National Science Foundation, Grant No.; 0450696, The
Grainger Foundation, U.S.A.; NAFOSTED, Vietnam; Marie
Curie-IRSES/EPLANET, European Particle Physics Latin American Network,
European Union 7th Framework Program, Grant No. PIRSES-2009-GA-246806
and PIOF-GA-2013-624803; and UNESCO.; The Telescope Array experiment is
supported by the Japan Society for the Promotion of Science through
Grants-in-Aid for Scientific Research on Specially Promoted Research
(21000002) "Extreme Phenomena in the Universe Explored by Highest Energy
Cosmic Rays" and for Scientific Research (19104006), and the
Inter-University Research Program of the Institute for Cosmic Ray
Research; by the U.S. National Science Foundation awards PHY-0307098,
PHY-0601915, PHY-0649681, PHY-0703893, PHY-0758342, PHY-0848320,
PHY-1069280, PHY-1069286, PHY-1404495 and PHY-1404502; by the National
Research Foundation of Korea (2007-0093860, R32-10130, 2012R1A1A2008381,
2013004883); by the Russian Academy of Sciences, RFBR grants
11-02-01528a and 13-02-01311a (INR), IISN project No. 4.4502.13, and
Belgian Science Policy under IUAP VII/37 (ULB). The foundations of Dr.
Ezekiel R. and Edna Wattis Dumke, Willard L. Eccles, and George S. and
Dolores Dore Eccles all helped with generous donations. The State of
Utah supported the project through its Economic Development Board, and
the University of Utah through the Office of the Vice President for
Research. The experimental site became available through the cooperation
of the Utah School and Institutional Trust Lands Administration (SITLA),
U.S. Bureau of Land Management, and the U.S. Air Force. We also wish to
thank the people and the officials of Millard County, Utah for their
steadfast and warm support. We gratefully acknowledge the contributions
from the technical staffs of our home institutions. An allocation of
computer time from the Center for High Performance Computing at the
University of Utah is gratefully acknowledged.
NR 49
TC 5
Z9 5
U1 19
U2 55
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 JAN
PY 2016
IS 1
AR 037
DI 10.1088/1475-7516/2016/01/037
PG 34
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DD2EB
UT WOS:000369734300037
ER
PT J
AU White, OL
Umurhan, OM
Moore, JM
Howard, AD
AF White, Oliver L.
Umurhan, Orkan M.
Moore, Jeffrey M.
Howard, Alan D.
TI Modeling of ice pinnacle formation on Callisto
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Callisto; pinnacle; sublimation; ice; modeling
ID GALILEAN SATELLITES; WATER-ICE; SIMULATION-MODEL; SURFACE; STABILITY;
DEGRADATION; SUBLIMATION; GANYMEDE; REGION; MOON
AB Callisto's pinnacle terrain has been interpreted to form through sublimation weathering of bedrock and subsequent deposition of the sublimated ice in local cold traps on peaks and crater rims. To investigate how these processes are affected by environmental parameters, including solar illumination and the composition and concentration of ices in the crust, we employ the MARSSIM landform evolution model and advance its treatment of the physics that underlies the relevant processes. Both ice sublimation and deposition are controlled by surface temperature, which we calculate based on energy contributions from both insolation and thermal reradiation from the surrounding landscape. We perform 4.5Gyr duration simulations whereby we separately consider and model CO2 and H2O as the crustal ice species. We find that sublimating a crustal content of 10% CO2 ice (a reasonable but arbitrarily selected value) yields present-day landform degradation and regolith coverage that is comparable to what is observed on Callisto. In our H2O ice simulations we reproduce the essential features of pinnacle ice distribution at both the equator and midlatitudes. Our present nominal crustal H2O ice content is 33%, which produces a maximum pinnacle ice thickness of 64m. Pinnacle height is likely limited by collapse or mass wasting of the ice once it reaches a certain thickness.
C1 [White, Oliver L.; Umurhan, Orkan M.; Moore, Jeffrey M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Howard, Alan D.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
RP White, OL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM oliver.l.white@nasa.gov
FU Outer Planets Research Program fund; NASA
FX We would like to acknowledge the Outer Planets Research Program fund
entitled "Exogenic Landform and Surface Texture Evolution on Icy
Satellites," as well as the NASA Postdoctoral Program (administered by
Oak Ridge Associated Universities), for providing the funding necessary
to accomplish this study. We would also like to thank Dale Cruikshank
and Luis Teodoro for helpful advice regarding our thermal model and ice
deposition routine and Paul Schenk for providing us with ISIS cube files
of Galileo imaging of Callisto. Details of certain routines that are
implemented in our model are included in Text S1 of the supporting
information. Any requests for data used in this study should be sent to
Oliver White at oliver.l.white@nasa.gov.
NR 56
TC 0
Z9 0
U1 1
U2 4
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 JAN
PY 2016
VL 121
IS 1
BP 21
EP 45
DI 10.1002/2015JE004846
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DD8LD
UT WOS:000370177100002
ER
PT J
AU Francois, P
Szopa, C
Buch, A
Coll, P
McAdam, AC
Mahaffy, PR
Freissinet, C
Glavin, DP
Navarro-Gonzalez, R
Cabane, M
AF Francois, P.
Szopa, C.
Buch, A.
Coll, P.
McAdam, A. C.
Mahaffy, P. R.
Freissinet, C.
Glavin, D. P.
Navarro-Gonzalez, R.
Cabane, M.
TI Magnesium sulfate as a key mineral for the detection of organic
molecules on Mars using pyrolysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE pyrolysis; organic molecules; magnesium sulfate; perchlorate; Mars
Science Laboratory; Sample Analysis at Mars
ID THERMAL-DECOMPOSITION; GALE CRATER; MASS-SPECTROMETRY; PERCHLORATE;
MATTER; SOILS; EVOLUTION; ASTEROIDS; PHTHALATE; SURFACE
AB Pyrolysis of soil or rock samples is the preferred preparation technique used on Mars to search for organic molecules up today. During pyrolysis, oxichlorines present in the soil of Mars release oxidant species that alter the organic molecules potentially contained in the samples collected by the space probes. This process can explain the difficulty experienced by in situ exploration probes to detect organic materials in Mars soil samples until recently. Within a few months, the Curiosity rover should reach and analyze for the first time soils rich in sulfates which could induce a different behavior of the organics during the pyrolysis compared with the types of soils analyzed up today. For this reason, we systematically studied the pyrolysis of organic molecules trapped in magnesium sulfate, in the presence or absence of calcium perchlorate. Our results show that organics trapped in magnesium sulfate can undergo some oxidation and sulfuration during the pyrolysis. But these sulfates are also shown to protect organics trapped inside the crystal lattice and/or present in fluid inclusions from the oxidation induced by the decomposition of calcium perchlorate and probably other oxychlorine phases currently detected on Mars. Trapped organics may also be protected from degradation processes induced by other minerals present in the sample, at least until these organics are released from the pyrolyzed sulfate mineral (similar to 700 degrees C in our experiment). Hence, we suggest magnesium sulfate as one of the minerals to target in priority for the search of organic molecules by the Curiosity and ExoMars 2018 rovers.
C1 [Francois, P.; Coll, P.] Univ Paris 07, CNRS, Lab Interuniv Syst Atmospher, UMR 7583, Creteil, France.
[Francois, P.; Coll, P.] Univ Paris Est Creteil, Creteil, France.
[Szopa, C.; Cabane, M.] Univ Versailles St Quentin, Guyancourt, France.
[Szopa, C.; Cabane, M.] Univ Paris 06, Sorbonne Univ, CNRS INSU, Guyancourt, France.
[Szopa, C.; Cabane, M.] LATMOS IPSL, Guyancourt, France.
[Buch, A.] Ecole Cent Paris, Lab Genie Proc & Mat, Chatenay Malabry, France.
[McAdam, A. C.; Mahaffy, P. R.; Glavin, D. P.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD USA.
[Freissinet, C.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD USA.
[Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
RP Francois, P (reprint author), Univ Paris 07, CNRS, Lab Interuniv Syst Atmospher, UMR 7583, Creteil, France.; Francois, P (reprint author), Univ Paris Est Creteil, Creteil, France.
EM pascaline.francois@lisa.u-pec.fr
RI Gonzalez, Rafael/D-1748-2009; Glavin, Daniel/D-6194-2012; szopa,
cyril/C-6865-2015
OI Glavin, Daniel/0000-0001-7779-7765; szopa, cyril/0000-0002-0090-4056
FU French Space Agency (CNES); Institut Universitaire de France (IUF)
FX All data used in this paper are available at the Laboratoire
Interuniversitaire des Systemes Atmosperique by requests. SAM-GC team
acknowledges support from the French Space Agency (CNES) and Institut
Universitaire de France (IUF). We also thank Brad Sutter for his help
and comments on this paper.
NR 49
TC 2
Z9 2
U1 12
U2 29
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 JAN
PY 2016
VL 121
IS 1
BP 61
EP 74
DI 10.1002/2015JE004884
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DD8LD
UT WOS:000370177100004
ER
PT J
AU Treiman, AH
Bish, DL
Vaniman, DT
Chipera, SJ
Blake, DF
Ming, DW
Morris, RV
Bristow, TF
Morrison, SM
Baker, MB
Rampe, EB
Downs, RT
Filiberto, J
Glazner, AF
Gellert, R
Thompson, LM
Schmidt, ME
Le Deit, L
Wiens, RC
McAdam, AC
Achilles, CN
Edgett, KS
Farmer, JD
Fendrich, KV
Grotzinger, JP
Gupta, S
Morookian, JM
Newcombe, ME
Rice, MS
Spray, JG
Stolper, EM
Sumner, DY
Vasavada, AR
Yen, AS
AF Treiman, Allan H.
Bish, David L.
Vaniman, David T.
Chipera, Steve J.
Blake, David F.
Ming, Doug W.
Morris, Richard V.
Bristow, Thomas F.
Morrison, Shaunna M.
Baker, Michael B.
Rampe, Elizabeth B.
Downs, Robert T.
Filiberto, Justin
Glazner, Allen F.
Gellert, Ralf
Thompson, Lucy M.
Schmidt, Mariek E.
Le Deit, Laetitia
Wiens, Roger C.
McAdam, Amy C.
Achilles, Cherie N.
Edgett, Kenneth S.
Farmer, Jack D.
Fendrich, Kim V.
Grotzinger, John P.
Gupta, Sanjeev
Morookian, John Michael
Newcombe, Megan E.
Rice, Melissa S.
Spray, John G.
Stolper, Edward M.
Sumner, Dawn Y.
Vasavada, Ashwin R.
Yen, Albert S.
TI Mineralogy, provenance, and diagenesis of a potassic basaltic sandstone
on Mars: CheMin X-ray diffraction of the Windjana sample (Kimberley
area, Gale Crater)
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; CheMin; MSL; Windjana; sandstone; X-ray diffraction
ID NORTHWEST AFRICA 7034; A-TYPE GRANITES; ALKALINE MAGMATISM;
CRYSTAL-STRUCTURE; STRUCTURAL STATE; MARTIAN MANTLE;
MOSSBAUER-SPECTROSCOPY; SOUTHERN CALIFORNIA; CATION DISTRIBUTION;
SEDIMENTARY-ROCKS
AB The Windjana drill sample, a sandstone of the Dillinger member (Kimberley formation, Gale Crater, Mars), was analyzed by CheMin X-ray diffraction (XRD) in the MSL Curiosity rover. From Rietveld refinements of its XRD pattern, Windjana contains the following: sanidine (21% weight, similar to Or(95)); augite (20%); magnetite (12%); pigeonite; olivine; plagioclase; amorphous and smectitic material (similar to 25%); and percent levels of others including ilmenite, fluorapatite, and bassanite. From mass balance on the Alpha Proton X-ray Spectrometer (APXS) chemical analysis, the amorphous material is Fe rich with nearly no other cationslike ferrihydrite. The Windjana sample shows little alteration and was likely cemented by its magnetite and ferrihydrite. From ChemCam Laser-Induced Breakdown Spectrometer (LIBS) chemical analyses, Windjana is representative of the Dillinger and Mount Remarkable members of the Kimberley formation. LIBS data suggest that the Kimberley sediments include at least three chemical components. The most K-rich targets have 5.6% K2O, similar to 1.8 times that of Windjana, implying a sediment component with >40% sanidine, e.g., a trachyte. A second component is rich in mafic minerals, with little feldspar (like a shergottite). A third component is richer in plagioclase and in Na2O, and is likely to be basaltic. The K-rich sediment component is consistent with APXS and ChemCam observations of K-rich rocks elsewhere in Gale Crater. The source of this sediment component was likely volcanic. The presence of sediment from many igneous sources, in concert with Curiosity's identifications of other igneous materials (e.g., mugearite), implies that the northern rim of Gale Crater exposes a diverse igneous complex, at least as diverse as that found in similar-age terranes on Earth.
C1 [Treiman, Allan H.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Bish, David L.; Achilles, Cherie N.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Vaniman, David T.] Planetary Sci Inst, Tucson, AZ USA.
[Chipera, Steve J.] Chesapeake Energy Corp, Oklahoma City, OK USA.
[Blake, David F.; Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ming, Doug W.; Morris, Richard V.; Rampe, Elizabeth B.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Div, Houston, TX USA.
[Morrison, Shaunna M.; Downs, Robert T.; Fendrich, Kim V.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Baker, Michael B.; Grotzinger, John P.; Newcombe, Megan E.; Stolper, Edward M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Filiberto, Justin] So Illinois Univ, Dept Geol, Carbondale, IL 62901 USA.
[Glazner, Allen F.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC USA.
[Gellert, Ralf] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Thompson, Lucy M.; Spray, John G.] Univ New Brunswick, Dept Earth Sci, Fredericton, NB, Canada.
[Schmidt, Mariek E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada.
[Le Deit, Laetitia] LPGN CNRS, UMR6112, Lab Planetol & Geodynam Nantes, Nantes, France.
[Le Deit, Laetitia] Univ Nantes, Nantes, France.
[Wiens, Roger C.] Los Alamos Natl Lab, Space Remote Sensing, Los Alamos, NM USA.
[McAdam, Amy C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Edgett, Kenneth S.] Malin Space Sci Syst Inc, San Diego, CA USA.
[Farmer, Jack D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Gupta, Sanjeev] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England.
[Morookian, John Michael; Vasavada, Ashwin R.; Yen, Albert S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rice, Melissa S.] Western Washington Univ, Dept Earth Sci, Bellingham, WA 98225 USA.
[Sumner, Dawn Y.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
RP Treiman, AH (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
EM treiman@lpi.usra.edu
FU NASA
FX The authors are grateful to the whole MSL Curiosity team, both engineers
and scientists, who have made the mission possible and these data
available. We are particularly grateful to the engineers who designed
and built CheMin, the drill system (SA/SpAH), and the CHIMRA
sieve/delivery system. Primary data used here are publically available
through the NASA Planetary Data System (https://pds.nasa.gov);
additional data are in the supporting information and from the authors.
We are grateful to S. Potter-McIntyre, D. Baratoux (Associate Editor),
and two anonymous reviewers for insightful and helpful critiques. NASA
funded this research via contracts with the Jet Propulsion Laboratory,
California Institute of Technology; part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. Naming of commercial products or software packages is
for documentation, and does not constitute endorsement by NASA, JPL, or
the authors. LPI Contribution 1888.
NR 187
TC 18
Z9 18
U1 11
U2 41
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 JAN
PY 2016
VL 121
IS 1
BP 75
EP 106
DI 10.1002/2015JE004932
PG 32
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DD8LD
UT WOS:000370177100005
ER
PT J
AU Collow, AB
Ghate, VP
Miller, MA
Trabachino, LC
AF Collow, Allison B.
Ghate, Virendra P.
Miller, Mark A.
Trabachino, Lynne C.
TI A one-year study of the diurnal cycle of meteorology, clouds and
radiation in the West African Sahel region
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE radiation budget; diurnal cycle; Saharan Air Layer; cloud radiative
effect; radiative flux divergence; West African Monsoon; lifting
condensation level
ID GEOSTATIONARY EARTH RADIATION; BUDGET GERB DATA; BOUNDARY-LAYER;
LONGWAVE RADIATION; WATER-VAPOR; PART II; MONSOON; PRECIPITATION;
CLIMATE; SEASON
AB The diurnal cycles of meteorological and radiation variables are analysed during the wet and dry seasons over the Sahel region of West Africa during 2006 using surface data collected by the Atmospheric Radiation Measurement (ARM) programme's Mobile Facility, satellite radiation measurements from the Geostationary Earth Radiation Budget (GERB) instrument aboard Meteosat 8, and reanalysis products from the National Centers for Environmental Prediction (NCEP). The meteorological analysis builds upon past studies of the diurnal cycle in the region by incorporating diurnal cycles of lower tropospheric wind profiles, thermodynamic profiles, integrated water vapour and liquid water measurements, and cloud radar measurements of frequency and location. These meteorological measurements are complemented by 3 h measurements of the diurnal cycles of the top-of-atmosphere (TOA) and surface short-wave (SW) and long-wave (LW) radiative fluxes and cloud radiative effects (CREs), and the atmospheric radiative flux divergence (RFD) and atmospheric CREs. Cirrus cloudiness during the dry season is shown to peak in coverage in the afternoon, while convective clouds during the wet season are shown to peak near dawn and have an afternoon minimum related to the rise of the lifting condensation level into the Saharan Air Layer. The LW and SW RFDs and CREs exhibit diurnal cycles during both seasons, but there is a relatively small difference in the LW cycles during the two seasons (10 - 30 W m(-2) depending on the variable and time of day). Small differences in the TOA CREs during the two seasons are overwhelmed by large differences in the surface SW CREs, which exceed 100 W m(-2). A significant surface SW CRE during the wet season combined with a negligible TOA SW CRE produces a diurnal cycle in the atmospheric CRE that is modulated primarily by the SW surface CRE, peaks at midday at approximate to 150 W m(-2), and varies widely from day to day.
C1 [Collow, Allison B.; Miller, Mark A.; Trabachino, Lynne C.] Rutgers State Univ, Inst Earth Ocean & Atmospher Sci, New Brunswick, NJ 08903 USA.
[Ghate, Virendra P.] Argonne Natl Lab, Div Environm Sci, Lemont, IL USA.
RP Collow, AB (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM allison.collow@nasa.gov
FU US Department of Energy Office of Biological and Environmental Research
[DE-FG02-08ER64531]; US Department of Energy's Atmospheric System
Research (ASR) Program, an Office of Science, Office of Biological and
Environmental Research [DE-AC02-06CH11357]
FX Our work is dedicated to the fond memory of Peter Lamb and Anthony
Slingo whose pioneering work in the Sahel region led to the current
study. We appreciate the work of the many scientists who assisted in the
deployment and data collection activates that resulted in the AMF-1 and
GERB datasets that are used in this study. We are particularly indebted
to Kim Nitschke for his work in deploying and operating the AMF-1,
Jacqueline Russell of Imperial College in London for helping us obtain
the GERB data, and Ashely Williamson for his support. This work is
funded by the US Department of Energy Office of Biological and
Environmental Research under grant number DE-FG02-08ER64531. Virendra
Ghate was supported by the US Department of Energy's Atmospheric System
Research (ASR) Program, an Office of Science, Office of Biological and
Environmental Research under the contract DE-AC02-06CH11357.
NR 63
TC 4
Z9 4
U1 2
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JAN
PY 2016
VL 142
IS 694
BP 16
EP 29
DI 10.1002/qj.2623
PN A
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD5QE
UT WOS:000369978300002
ER
PT J
AU Healey, NC
Oberbauer, SF
Hollister, RD
AF Healey, Nathan C.
Oberbauer, Steven F.
Hollister, Robert D.
TI Examination of Surface Temperature Modification by Open-Top Chambers
along Moisture and Latitudinal Gradients in Arctic Alaska Using Thermal
Infrared Photography
SO REMOTE SENSING
LA English
DT Article
DE remote sensing; thermal imagery; open-top chamber; Arctic; Alaska
ID INTERNATIONAL TUNDRA EXPERIMENT; SUMMER TEMPERATURE; PLANT COMMUNITY;
RESPONSES; TERM; CO2; MANIPULATION; ECOSYSTEMS; FLUXES; SOILS
AB Passive warming manipulation methodologies, such as open-top chambers (OTCs), are a meaningful approach for interpretation of impacts of climate change on the Arctic tundra biome. The magnitude of OTC warming has been studied extensively, revealing an average plot-level warming of air temperature that ranges between 1 and 3 degrees C as measured by shielded resistive sensors or thermocouples. Studies have also shown that the amount of OTC warming depends in part on location climate, vegetation, and soil properties. While digital infrared thermometers have been employed in a few comparisons, most of the focus of the effectiveness of OTC warming has been on air or soil temperature rather than tissue or surface temperatures, which directly translate to metabolism. Here we used thermal infrared (TIR) photography to quantify tissue and surface temperatures and their spatial variability at a previously unavailable resolution (3-6 mm(2)). We analyzed plots at three locations that are part of the International Tundra Experiment (ITEX)-Arctic Observing Network (AON-ITEX) network along both moisture and latitudinal gradients spanning from the High Arctic (Barrow, AK, USA) to the Low Arctic (Toolik Lake, AK, USA). Our results show a range of OTC surface warming from 2.65 to 1.27 degrees C (31%-10%) at our three sites. The magnitude of surface warming detected by TIR imagery in this study was comparable to increases in air temperatures previously reported for these sites. However, the thermal images revealed wide ranges of surface temperatures within the OTCs, with some surfaces well above ambient unevenly distributed within the plots under sunny conditions. We note that analyzing radiometric temperature may be an alternative for future studies that examine data acquired at the same time of day from sites that are in close geographic proximity to avoid the requirement of emissivity or atmospheric correction for validation of results. We foresee future studies using TIR photography to describe species-level thermodynamics that could prove highly valuable toward a better understanding of species-specific responses to climate change in the Arctic.
C1 [Healey, Nathan C.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Oberbauer, Steven F.] Florida Int Univ, Dept Biol Sci, 11200 SW 8th St, Miami, FL 33199 USA.
[Hollister, Robert D.] Grand Valley State Univ, Dept Biol Sci, 212 Henry Hall,1 Campus Dr, Allendale, MI 49401 USA.
RP Healey, NC (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nhealey@jpl.nasa.gov; oberbaue@fiu.edu; hollistr@gvsu.edu
OI Goossens, Alain/0000-0002-1599-551X
FU National Science Foundation [OPP-0856710, OPP-0856516, PLR-1432982,
PLR-1432277]; National Aeronautics and Space Administration
FX This material is based in part upon work supported by the National
Science Foundation under Grant Numbers OPP-0856710, OPP-0856516,
PLR-1432982, and PLR-1432277. Any opinions, findings, and conclusions or
recommendations expressed in this material are those of the author(s)
and do not necessarily reflect the views of the National Science
Foundation. The authors acknowledge the following for assistance in this
research: Timothy Botting, Jeremy May, and Christine Pardo for aid in
field data collection, the Toolik Lake Biological Field Station Staff,
CH2MHill Polar Services, and UMIAQ Logistics. The authors of this
manuscript also graciously acknowledge the independent peer reviewers
for improving the quality of this manuscript. Additional support for
Nathan C. Healey was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 31
TC 0
Z9 0
U1 3
U2 22
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2016
VL 8
IS 1
AR 54
DI 10.3390/rs8010054
PG 19
WC Remote Sensing
SC Remote Sensing
GA DC8UF
UT WOS:000369494500039
ER
PT J
AU Li, YH
Wu, AS
Xiong, XX
AF Li, Yonghong
Wu, Aisheng
Xiong, Xiaoxiong
TI Inter-Comparison of S-NPP VIIRS and Aqua MODIS Thermal Emissive Bands
Using Hyperspectral Infrared Sounder Measurements as a Transfer
Reference
SO REMOTE SENSING
LA English
DT Article
DE VIIRS; MODIS; AIRS; CrIS; thermal emissive bands; calibration
AB This paper compares the calibration consistency of the spectrally-matched thermal emissive bands (TEB) between the Suomi National Polar-orbiting Partnership (S-NPP) Visible Infrared Imaging Radiometer Suite (VIIRS) and the Aqua Moderate Resolution Imaging Spectroradiometer (MODIS), using observations from their simultaneous nadir overpasses (SNO). Nearly-simultaneous hyperspectral measurements from the Aqua Atmospheric Infrared Sounder(AIRS) and the S-NPP Cross-track Infrared Sounder (CrIS) are used to account for existing spectral response differences between MODIS and VIIRS TEB. The comparison uses VIIRS Sensor Data Records (SDR) in MODIS five-minute granule format provided by the NASA Land Product and Evaluation and Test Element (PEATE) and Aqua MODIS Collection 6 Level 1 B (L1B) products. Each AIRS footprint of 13.5 km (or CrIS field of view of 14 km) is co-located with multiple MODIS (or VIIRS) pixels. The corresponding AIRS- and CrIS-simulated MODIS and VIIRS radiances are derived by convolutions based on sensor-dependent relative spectral response (RSR) functions. The VIIRS and MODIS TEB calibration consistency is evaluated and the two sensors agreed within 0.2 K in brightness temperature. Additional factors affecting the comparison such as geolocation and atmospheric water vapor content are also discussed in this paper.
C1 [Li, Yonghong; Wu, Aisheng] Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
RP Li, YH (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
EM yonghong.li@ssaihq.com; aisheng.wu@ssaihq.com;
xiaoxiong.xiong-1@nasa.gov
NR 22
TC 0
Z9 0
U1 2
U2 7
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2016
VL 8
IS 1
AR 72
DI 10.3390/rs8010072
PG 14
WC Remote Sensing
SC Remote Sensing
GA DC8UF
UT WOS:000369494500014
ER
PT J
AU McIntire, J
Moyer, D
Oudrari, H
Xiong, X
AF McIntire, Jeff
Moyer, David
Oudrari, Hassan
Xiong, Xiaoxiong
TI Pre-Launch Radiometric Characterization of JPSS-1 VIIRS Thermal Emissive
Bands
SO REMOTE SENSING
LA English
DT Article
DE JPSS; VIIRS; calibration; pre-launch; thermal bands
ID MODIS
AB Pre-launch characterization and calibration of the thermal emissive spectral bands on the Joint Polar Satellite System (JPSS-1) Visible Infrared Imaging Radiometer Suite (VIIRS) is critical to ensure high quality data products for environmental and climate data records post-launch. A comprehensive test program was conducted at the Raytheon El Segundo facility in 2013-2014, including extensive environmental testing. This work is focused on the thermal band radiometric performance and stability, including evaluation of a number of sensor performance metrics and estimation of uncertainties. Analysis has shown that JPSS-1 VIIRS thermal bands perform very well in relation to their design specifications, and comparisons to the Suomi National Polar-orbiting Partnership (SNPP) VIIRS instrument have shown their performance to be comparable.
C1 [McIntire, Jeff; Oudrari, Hassan] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Moyer, David] Aerosp Corp, El Segundo, CA 90245 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McIntire, J (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM jeffrey.mcintire@ssaihq.com; david.i.moyer@noaa.gov;
Hassan.oudrari@ssaihq.com; xiaoxiong.xiong-1@nasa.gov
NR 16
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2016
VL 8
IS 1
AR 47
DI 10.3390/rs8010047
PG 19
WC Remote Sensing
SC Remote Sensing
GA DC8UF
UT WOS:000369494500029
ER
PT J
AU Oudrari, H
McIntire, J
Xiong, XX
Butler, J
Ji, Q
Schwarting, T
Lee, SY
Efremova, B
AF Oudrari, Hassan
McIntire, Jeff
Xiong, Xiaoxiong
Butler, James
Ji, Qiang
Schwarting, Thomas
Lee, Shihyan
Efremova, Boryana
TI JPSS-1 VIIRS Radiometric Characterization and Calibration Based on
Pre-Launch Testing
SO REMOTE SENSING
LA English
DT Article
DE JPSS; SNPP; VIIRS; pre-launch; radiometric; performance; calibration;
spectral
ID PRODUCTS; MODIS; LAND
AB The Visible Infrared Imaging Radiometer Suite (VIIRS) on-board the first Joint Polar Satellite System (JPSS) completed its sensor level testing on December 2014. The JPSS-1 (J1) mission is scheduled to launch in December 2016, and will be very similar to the Suomi-National Polar-orbiting Partnership (SNPP) mission. VIIRS instrument has 22 spectral bands covering the spectrum between 0.4 and 12.6 m. It is a cross-track scanning radiometer capable of providing global measurements twice daily, through observations at two spatial resolutions, 375 m and 750 m at nadir for the imaging and moderate bands, respectively. This paper will briefly describe J1 VIIRS characterization and calibration performance and methodologies executed during the pre-launch testing phases by the government independent team to generate the at-launch baseline radiometric performance and the metrics needed to populate the sensor data record (SDR) Look-Up-Tables (LUTs). This paper will also provide an assessment of the sensor pre-launch radiometric performance, such as the sensor signal to noise ratios (SNRs), radiance dynamic range, reflective and emissive bands calibration performance, polarization sensitivity, spectral performance, response-vs-scan (RVS), and scattered light response. A set of performance metrics generated during the pre-launch testing program will be compared to both the VIIRS sensor specification and the SNPP VIIRS pre-launch performance.
C1 [Oudrari, Hassan; McIntire, Jeff; Ji, Qiang; Schwarting, Thomas; Lee, Shihyan; Efremova, Boryana] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong; Butler, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lee, Shihyan] SAIC, Beltsville, MD 20705 USA.
[Efremova, Boryana] Earth Resources Technol Inc, Silver Spring, MD 20707 USA.
RP Oudrari, H (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM Hassan.oudrari-1@nasa.gov; jeffrey.mcintire@ssaihq.com;
xiaoxiong.xiong-1@nasa.gov; james.j.butler@nasa.gov;
qiang.ji@ssaihq.com; thomas.schwarting@ssaihq.com; shihyan.lee@nasa.gov;
boryana.efremova@noaa.gov
NR 22
TC 6
Z9 6
U1 1
U2 2
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2016
VL 8
IS 1
AR 41
DI 10.3390/rs8010041
PG 20
WC Remote Sensing
SC Remote Sensing
GA DC8UF
UT WOS:000369494500022
ER
PT J
AU Wang, ZP
Xiong, XX
Li, YH
AF Wang, Zhipeng
Xiong, Xiaoxiong
Li, Yonghong
TI Improved Band-to-Band Registration Characterization for VIIRS Reflective
Solar Bands Based on Lunar Observations
SO REMOTE SENSING
LA English
DT Article
DE VIIRS; band-to-band registration; Moon; spatial characterization
ID ORBIT SPATIAL CHARACTERIZATION; MOON; PERFORMANCE
AB Spectral bands of the Visible Infrared Imaging Radiometer Suite (VIIRS) instrument aboard the Suomi National Polar-orbiting Partnership (S-NPP) satellite are spatially co-registered. The accuracy of the band-to-band registration (BBR) is one of the key spatial parameters that must be characterized. Unlike its predecessor, the Moderate Resolution Imaging Spectroradiometer (MODIS), VIIRS has no on-board calibrator specifically designed to perform on-orbit BBR characterization. To circumvent this problem, a BBR characterization method for VIIRS reflective solar bands (RSB) based on regularly-acquired lunar images has been developed. While its results can satisfactorily demonstrate that the long-term stability of the BBR is well within +/- 0.1 moderate resolution band pixels, undesired seasonal oscillations have been observed in the trending. The oscillations are most obvious between the visible/near-infrared bands and short-/middle wave infrared bands. This paper investigates the oscillations and identifies their cause as the band/spectral dependence of the centroid position and the seasonal rotation of the lunar images over calibration events. Accordingly, an improved algorithm is proposed to quantify the rotation and compensate for its impact. After the correction, the seasonal oscillation in the resulting BBR is reduced from up to 0.05 moderate resolution band pixels to around 0.01 moderate resolution band pixels. After removing this spurious seasonal oscillation, the BBR, as well as its long-term drift are well determined.
C1 [Wang, Zhipeng; Li, Yonghong] Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Greenbelt, MD 20706 USA.
[Xiong, Xiaoxiong] NASA GSFC, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
RP Wang, ZP (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Greenbelt, MD 20706 USA.
EM zhipeng.wang@ssaihq.com; xiaoxiong.xiong-1@nasa.gov;
yonghong.li@ssaihq.com
OI Li, Yuan/0000-0001-5141-8456; Wang, Zhipeng/0000-0002-9108-9009
NR 17
TC 4
Z9 4
U1 1
U2 2
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2016
VL 8
IS 1
AR 27
DI 10.3390/rs8010027
PG 12
WC Remote Sensing
SC Remote Sensing
GA DC8US
UT WOS:000369495800026
ER
PT J
AU Diaz-Santos, T
Assef, RJ
Blain, AW
Tsai, CW
Aravena, M
Eisenhardt, P
Wu, J
Stern, D
Bridge, C
AF Diaz-Santos, T.
Assef, R. J.
Blain, A. W.
Tsai, C. -W.
Aravena, M.
Eisenhardt, P.
Wu, J.
Stern, D.
Bridge, C.
TI THE STRIKINGLY UNIFORM, HIGHLY TURBULENT INTERSTELLAR MEDIUM OF THE MOST
LUMINOUS GALAXY IN THE UNIVERSE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: ISM; galaxies: nuclei; galaxies: starburst; infrared: galaxies
ID C II EMISSION; POLYCYCLIC AROMATIC-HYDROCARBONS; DUST-OBSCURED GALAXIES;
BLACK-HOLE ACCRETION; STAR-FORMATION RATE; 10(8) SOLAR MASS; HOST
GALAXIES; SUBMILLIMETER GALAXIES; INFRARED GALAXIES; STARBURST GALAXY
AB Observed at z = 4.601 and with L-bol = 3.5 x 10(14) L-circle dot, W2246-0526 is the most luminous galaxy known in the universe. and hosts a deeply buried active galactic nucleus (AGN)/supermassive black hole (SMBH). Discovered using the Wide-field Infrared Survey Explorer, W2246-0526 is classified as a hot dust-obscured galaxy, based on its luminosity and dust temperature. Here, we present spatially resolved ALMA [C-II] 157.7 mu m observations of W2246-0526, providing unique insight into the kinematics of its interstellar medium (ISM). The measured [C-II]-to-far-infrared ratio is similar to 2 x 10(-4), implying ISM conditions that compare only with the most obscured, compact starbursts and AGNs in the local universe today. The spatially resolved [C-II] line is strikingly uniform and very broad, 500-600 km s(-1) wide, extending throughout the entire galaxy over about 2.5 kpc, with modest shear. Such a large, homogeneous velocity dispersion indicates a highly turbulent medium. W2246-0526 is unstable in terms of the energy and momentum that are being injected into the ISM, strongly suggesting that the gas is being blown away from the system isotropically, likely reflecting a cathartic state on its road to becoming an unobscured quasar. W2246-0526 provides an extraordinary laboratory to study and model the properties and kinematics of gas in an extreme environment under strong feedback, at a time when the universe was 1/10 of its current age: a system pushing the limits that can be reached during galaxy formation.
C1 [Diaz-Santos, T.; Assef, R. J.; Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito Libertador 441, Santiago, Chile.
[Blain, A. W.] Univ Leicester, Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
[Tsai, C. -W.; Eisenhardt, P.; Stern, D.; Bridge, C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wu, J.] Univ Calif Los Angeles, Div Phys & Astron, Phys & Astron Bldg,430 Portola Plaza, Los Angeles, CA 90095 USA.
RP Diaz-Santos, T (reprint author), Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito Libertador 441, Santiago, Chile.
EM tanio.diaz@mail.udp.cl
FU ALMA-CONICYT [31130005]; FONDECYT [1151239, 1151408, 1140099];
Gemini-CONICYT [32120009]
FX The authors would like to thank H. Jun for suggestions provided during
the analysis of the data. T.D.-S. acknowledges support from ALMA-CONICYT
project 31130005 and FONDECYT 1151239. R.J.A. acknowledges support from
Gemini-CONICYT project 32120009 and FONDECYT 1151408. The work of
C.-W.T., P.E., D.S., and C.B. was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. M.A. acknowledges partial support from FONDECYT through grant
1140099. 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.
NR 44
TC 8
Z9 8
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 1
PY 2016
VL 816
IS 1
AR L6
DI 10.3847/2041-8205/816/1/L6
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AE
UT WOS:000369369900006
ER
PT J
AU Fox, OD
Johansson, J
Kasliwal, M
Andrews, J
Bally, J
Bond, HE
Boyer, ML
Gehrz, RD
Helou, G
Hsiao, EY
Masci, FJ
Parthasarathy, M
Smith, N
Tinyanont, S
Van Dyk, SD
AF Fox, Ori D.
Johansson, Joel
Kasliwal, Mansi
Andrews, Jennifer
Bally, John
Bond, Howard E.
Boyer, Martha L.
Gehrz, R. D.
Helou, George
Hsiao, E. Y.
Masci, Frank J.
Parthasarathy, M.
Smith, Nathan
Tinyanont, Samaporn
Van Dyk, Schuyler D.
TI AN EXCESS OF MID-INFRARED EMISSION FROM THE TYPE Iax SN 2014dt
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; dust, extinction; infrared: stars; supernovae:
general; supernovae: individual (SN 2014dt)
ID CORE-COLLAPSE SUPERNOVA; SPITZER-SPACE-TELESCOPE; PTF 11KX; DUST;
ENVELOPE; SPECTRA; 2005HK; 2012Z; SPEED
AB Supernovae Type Iax (SNe Iax) are less energetic and less luminous than typical thermonuclear explosions. A suggested explanation for the observed characteristics of this subclass is a binary progenitor system consisting of a CO white dwarf primary accreting from a helium star companion. A single-degenerate explosion channel might be expected to result in a dense circumstellar medium (CSM), although no evidence for such a CSM has yet been observed for this subclass. Here we present recent Spitzer. observations of the SN Iax 2014dt obtained by the SPIRITS program nearly one year post-explosion that reveal a strong mid-IR excess over the expected fluxes of more normal SNe Ia. This excess is consistent with 10(-5)M(circle dot) of newly formed dust, which would be the first time that newly formed dust has been observed to form in a Type Ia. The excess, however, is also consistent with a dusty CSM that was likely formed in pre-explosion mass-loss, thereby suggesting a single degenerate progenitor system. Compared to other SNe Ia that show significant shock interaction (SNe Ia-CSM) and interacting corecollapse events (SNe IIn), this dust shell in SN 2014dt is less massive. We consider the implications that such a pre-existing dust shell has for the progenitor system, including a binary system with a mass donor that is a red giant, a red supergiant, or an asymptotic giant branch star.
C1 [Fox, Ori D.; Bond, Howard E.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Johansson, Joel] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Kasliwal, Mansi; Tinyanont, Samaporn] CALTECH, Pasadena, CA 91125 USA.
[Andrews, Jennifer; Smith, Nathan] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Bally, John] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80389 USA.
[Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Boyer, Martha L.] NASA, Goddard Space Flight Ctr, CRESST, Code 665, Greenbelt, MD 20771 USA.
[Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, Martha L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gehrz, R. D.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA.
[Helou, George; Masci, Frank J.; Van Dyk, Schuyler D.] CALTECH, IPAC, Mailcode 100-22, Pasadena, CA 91125 USA.
[Hsiao, E. Y.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Parthasarathy, M.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
RP Fox, OD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM ofox@stsci.edu
OI Van Dyk, Schuyler/0000-0001-9038-9950
FU Spitzer Space Telescope [11063]; NASA; NASA through JPL/Caltech
FX This work is based on data obtained via Program #11063 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 authors thank Ryan Foley for useful discussions. We
thank Peter Milne, Jacob Jencson, and Tom Prince for help with
observations.
NR 42
TC 3
Z9 3
U1 1
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 1
PY 2016
VL 816
IS 1
AR L13
DI 10.3847/2041-8205/816/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AE
UT WOS:000369369900013
ER
PT J
AU Jennings, DE
Cottini, V
Nixon, CA
Achterberg, RK
Flasar, FM
Kunde, VG
Romani, PN
Samuelson, RE
Mamoutkine, A
Gorius, NJP
Coustenis, A
Tokano, T
AF Jennings, D. E.
Cottini, V.
Nixon, C. A.
Achterberg, R. K.
Flasar, F. M.
Kunde, V. G.
Romani, P. N.
Samuelson, R. E.
Mamoutkine, A.
Gorius, N. J. P.
Coustenis, A.
Tokano, T.
TI SURFACE TEMPERATURES ON TITAN DURING NORTHERN WINTER AND SPRING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE infrared: planetary systems; planets and satellites: individual (Titan);
radiation mechanisms: thermal; radiative transfer
ID COMPOSITE INFRARED SPECTROMETER; CASSINI RADIO OCCULTATIONS; ATMOSPHERE;
CIRCULATION; SPECTRA; MIDDLE; STRATOSPHERE; TROPOSPHERE; DYNAMICS
AB Meridional brightness temperatures were measured on the surface of Titan during the 2004-2014 portion of the Cassini mission by the Composite Infrared Spectrometer. Temperatures mapped from pole to pole during five two-year periods show a marked seasonal dependence. The surface temperature near the south pole over this time decreased by 2 K from 91.7 +/- 0.3 to 89.7 +/- 0.5 K while at the north pole the temperature increased by 1 K from 90.7 +/- 0.5 to 91.5 +/- 0.2 K. The latitude of maximum temperature moved from 19 S to 16 N, tracking the subsolar latitude. As the latitude changed, the maximum temperature remained constant at 93.65 +/- 0.15 K. In 2010 our temperatures repeated the north-south symmetry seen by Voyager one Titan year earlier in 1980. Early in the mission, temperatures at all latitudes had agreed with GCM predictions, but by 2014 temperatures in the north were lower than modeled by 1 K. The temperature rise in the north may be delayed by cooling of sea surfaces and moist ground brought on by seasonal methane precipitation and evaporation.
C1 [Jennings, D. E.; Cottini, V.; Nixon, C. A.; Achterberg, R. K.; Flasar, F. M.; Kunde, V. G.; Romani, P. N.; Samuelson, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cottini, V.; Achterberg, R. K.; Samuelson, R. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mamoutkine, A.] ADNET Syst Inc, Bethesda, MD 20817 USA.
[Gorius, N. J. P.] Catholic Univ Amer, Washington, DC 20064 USA.
[Coustenis, A.] Univ Paris 05, Univ Paris 06, Observ Paris, LESIA,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Tokano, T.] Univ Cologne, Albertus Magnus Pl, D-50923 Cologne, Germany.
RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM donald.e.jennings@nasa.gov
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012
OI Nixon, Conor/0000-0001-9540-9121;
FU NASA's Cassini mission and Cassini Data Analysis Program; DFG
[TO269/4-1]
FX The authors acknowledge support from NASA's Cassini mission and Cassini
Data Analysis Program. T.T. was supported by DFG Grant TO269/4-1. We
also thank A. Le Gall and M. Janssen for stimulating discussions and for
making available preprints of their work.
NR 38
TC 3
Z9 3
U1 1
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 1
PY 2016
VL 816
IS 1
AR L17
DI 10.3847/2041-8205/816/1/L17
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC7AE
UT WOS:000369369900017
ER
PT J
AU Gajbhiye, S
Meshram, C
Singh, SK
Srivastava, PK
Islam, T
AF Gajbhiye, Sarita
Meshram, Chandrashekhar
Singh, Sudhir Kumar
Srivastava, Prashant K.
Islam, Tanvir
TI Precipitation trend analysis of Sindh River basin, India, from 102-year
record (1901-2002)
SO ATMOSPHERIC SCIENCE LETTERS
LA English
DT Article
DE trend analysis; change-point analysis; annual rainfall series; Sindh
River basin
ID RAINFALL; PERFORMANCE; CLIMATE; TESTS
AB The study of long-term precipitation record is critically important for a country, whose food security and economy rely on the timely availability of water. In this study, the historical 102-year (1901-2002) rainfall data of the Sindh River basin (SRB), India, were analyzed for seasonal and annual trends. The Mann-Kendall test and Sen's slope model were used to identify the trend and the magnitude of the change, respectively. Spatial interpolation technique such as Kriging was used for interpolating the spatial pattern over SRB in GIS environment. The analysis revealed the significantly increasing precipitation trend in both seasonal and annual rainfall in the span of 102 years.
C1 [Gajbhiye, Sarita] Indian Inst Technol, Dept Water Resources Dev & Management, Roorkee, Uttar Pradesh, India.
[Meshram, Chandrashekhar] RTM Nagpur Univ, Dept Math, Nagpur, Maharashtra, India.
[Singh, Sudhir Kumar] Univ Allahabad, K Banerjee Ctr Atmospher & Ocean Studies, IIDS, Nehru Sci Ctr, Allahabad 211002, Uttar Pradesh, India.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt Rd, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi 221005, Uttar Pradesh, India.
[Islam, Tanvir] NOAA NESDIS Ctr Satellite Applicat & Res, College Pk, MD USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
RP Srivastava, PK (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt Rd, Greenbelt, MD 20771 USA.
EM prashant.k.srivastava@nasa.gov
FU Department of Science and Technology, Government of India
FX The first author would like to thanks the Department of Science and
Technology, Government of India for the financial support under the
scheme Innovation in Science Pursuit for Inspired Research (INSPIRE).
The views expressed here are those of the authors solely and do not
constitute a statement of policy, decision, or position on behalf of
NOAA/NASA or the authors' affiliated institutions.
NR 23
TC 0
Z9 0
U1 1
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1530-261X
J9 ATMOS SCI LETT
JI Atmos. Sci. Lett.
PD JAN
PY 2016
VL 17
IS 1
BP 71
EP 77
DI 10.1002/asl.602
PG 7
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA DD2FE
UT WOS:000369737200012
ER
PT J
AU Tang, H
Ganguly, S
Zhang, G
Hofton, MA
Nelson, RF
Dubayah, R
AF Tang, H.
Ganguly, S.
Zhang, G.
Hofton, M. A.
Nelson, R. F.
Dubayah, R.
TI Characterizing leaf area index (LAI) and vertical foliage profile (VFP)
over the United States
SO BIOGEOSCIENCES
LA English
DT Article
ID WAVE-FORM LIDAR; SIERRA NATIONAL FOREST; BIOMASS ESTIMATION; SPECIES
RICHNESS; LASER ALTIMETER; GLOBAL PRODUCTS; VEGETATION; CARBON;
ALGORITHM; MODIS
AB Leaf area index (LAI) and vertical foliage profile (VFP) are among the important canopy structural variables. Recent advances in lidar remote sensing technology have demonstrated the capability of accurately mapping LAI and VFP over large areas. The primary objective of this study was to derive and validate a LAI and VFP product over the contiguous United States (CONUS) using spaceborne waveform lidar data. This product was derived at the footprint level from the Geoscience Laser Altimeter System (GLAS) using a biophysical model. We validated GLAS-derived LAI and VFP across major forest biomes using airborne waveform lidar. The comparison results showed that GLAS retrievals of total LAI were generally accurate with little bias (r(2) = 0.67, bias = -0.13, RMSE = 0.75). The derivations of GLAS retrievals of VFP within layers were not as accurate overall (r(2) = 0.36, bias = -0.04, RMSE = 0.26), and these varied as a function of height, increasing from understory to overstory -0 to 5m layer: r(2) = 0.04, bias = 0.09, RMSE = 0.31; 10 to 15 m layer: r(2) = 0.53, bias = -0.08, RMSE = 0.22; and 15 to 20 m layer: r(2) = 0.66, bias = -0.05, RMSE = 0.20. Significant relationships were also found between GLAS LAI products and different environmental factors, in particular elevation and annual precipitation. In summary, our results provide a unique insight into vertical canopy structure distribution across North American ecosystems. This data set is a first step towards a baseline of canopy structure needed for evaluating climate and land use induced forest changes at the continental scale in the future, and should help deepen our understanding of the role of vertical canopy structure in terrestrial ecosystem processes across varying scales.
C1 [Tang, H.; Hofton, M. A.; Dubayah, R.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Ganguly, S.; Zhang, G.] NASA, BAERI, Ames Res Ctr, Moffett Field, CA USA.
[Nelson, R. F.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Code 618, Greenbelt, MD USA.
RP Tang, H (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM htang@umd.edu
RI Beckley, Matthew/D-4547-2013
FU NASA [NNX12AK07G]; Earth and Space Science graduate fellowship
[NNX12AN43H]
FX This work was funded by NASA under grant NNX12AK07G (Dubayah) and an
Earth and Space Science graduate fellowship, NNX12AN43H (Dubayah and
Tang). We thank Helen G. Cornejo and Wenli Huang for the raw LVIS
waveform process, and George Hurtt and Shunlin Liang for their advice on
product development. We also thank the NSIDC (National Snow & Ice Data
Center) User Services for their help on data acquisition and NASA Earth
Exchange (NEX) for computing resources.
NR 79
TC 3
Z9 3
U1 14
U2 26
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1726-4170
EI 1726-4189
J9 BIOGEOSCIENCES
JI Biogeosciences
PY 2016
VL 13
IS 1
BP 239
EP 252
DI 10.5194/bg-13-239-2016
PG 14
WC Ecology; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA DC9EN
UT WOS:000369524000016
ER
PT J
AU Campbell, JR
Ge, C
Wang, J
Welton, EJ
Bucholtz, A
Hyer, EJ
Reid, EA
Chew, BN
Liew, SC
Salinas, SV
Lolli, S
Kaku, KC
Lynch, P
Mahmud, M
Mohamad, M
Holben, BN
AF Campbell, James R.
Ge, Cui
Wang, Jun
Welton, Ellsworth J.
Bucholtz, Anthony
Hyer, Edward J.
Reid, Elizabeth A.
Chew, Boon Ning
Liew, Soo-Chin
Salinas, Santo V.
Lolli, Simone
Kaku, Kathleen C.
Lynch, Peng
Mahmud, Mastura
Mohamad, Maznorizan
Holben, Brent N.
TI Applying Advanced Ground-Based Remote Sensing in the Southeast Asian
Maritime Continent to Characterize Regional Proficiencies in Smoke
Transport Modeling
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Aerosols; Air quality; Lidars; Lidar observations; Radiosonde
observations; Regional models; Air pollution
ID AEROSOL OPTICAL DEPTH; TROPICAL TROPOPAUSE LAYER; GLOBAL CLIMATE MODELS;
DATA-ASSIMILATION; ATMOSPHERIC COMPOSITION; RADIATIVE IMPACT;
BOUNDARY-LAYER; UNITED-STATES; RAMAN LIDAR; EAST-ASIA
AB This work describes some of the most extensive ground-based observations of the aerosol profile collected in Southeast Asia to date, highlighting the challenges in simulating these observations with a mesoscale perspective. An 84-h WRF Model coupled with chemistry (WRF-Chem) mesoscale simulation of smoke particle transport at Kuching, Malaysia, in the southern Maritime Continent of Southeast Asia is evaluated relative to a unique collection of continuous ground-based lidar, sun photometer, and 4-h radiosonde profiling. The period was marked by relatively dry conditions, allowing smoke layers transported to the site unperturbed by wet deposition to be common regionally. The model depiction is reasonable overall. Core thermodynamics, including land/sea-breeze structure, are well resolved. Total model smoke extinction and, by proxy, mass concentration are low relative to observation. Smoke emissions source products are likely low because of undersampling of fires in infrared sun-synchronous satellite products, which is exacerbated regionally by endemic low-level cloud cover. Differences are identified between the model mass profile and the lidar profile, particularly during periods of afternoon convective mixing. A static smoke mass injection height parameterized for this study potentially influences this result. The model does not resolve the convective mixing of aerosol particles into the lower free troposphere or the enhancement of near-surface extinction from nighttime cooling and hygroscopic effects.
C1 [Campbell, James R.; Bucholtz, Anthony; Hyer, Edward J.; Reid, Elizabeth A.] US Navy, Res Lab, 7 Grace Hopper Ave Stop 2, Monterey, CA 93943 USA.
[Ge, Cui; Wang, Jun] Univ Nebraska, Dept Atmospher Sci, Lincoln, NE USA.
[Welton, Ellsworth J.; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Chew, Boon Ning; Liew, Soo-Chin; Salinas, Santo V.] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 117548, Singapore.
[Lolli, Simone] Joint Ctr Earth Syst Technol, Greenbelt, MD USA.
[Kaku, Kathleen C.; Lynch, Peng] Comp Sci Corp, Monterey, CA USA.
[Mahmud, Mastura] Natl Univ Malaysia, Bangi, Selangor, Malaysia.
[Mohamad, Maznorizan] Malaysian Meteorol Dept, Div Environm Studies, Petaling Jaya, Selangor, Malaysia.
RP Campbell, JR (reprint author), US Navy, Res Lab, 7 Grace Hopper Ave Stop 2, Monterey, CA 93943 USA.
EM james.campbell@nrlmry.navy.mil
RI Campbell, James/C-4884-2012; Hyer, Edward/E-7734-2011; Chew, Boon
Ning/M-2405-2016; Wang, Jun/A-2977-2008;
OI Campbell, James/0000-0003-0251-4550; Hyer, Edward/0000-0001-8636-2026;
Chew, Boon Ning/0000-0002-2933-7788; Wang, Jun/0000-0002-7334-0490; ge,
cui/0000-0002-6182-6856
FU Chief of Naval Research through the NRL Base Program [PE 0601153N];
Office of Naval Research [32 (PE 0602435N), 35 (PE 0602114N)]; NASA on
behalf of MPLNET [NNG13HH10I]; Southeast Asia Composition, Cloud,
Climate Coupling Regional Study (SEAC4RS) Science Team; NASA Radiation
Sciences Program; SEAC4RS Science Team; NASA Interdisciplinary Science
Program
FX Deployment of the Micro-Pulse Lidar Network (MPLNET) ALS, Aerosol
Robotic Network (AERONET) sun photometer, and Naval Research Laboratory
(NRL) radiation instrument package to Kuching during summer 2012 could
not have been achieved without the critical support and collaboration of
the Malaysian Meteorological Department (MMD), National University of
Malaysia, and National University of Singapore. Special thanks are given
to our MMD colleagues in Kuching, including State Director of Sarawak
MMD Wong Teck Kiong, Kuching Meteorological Observation Station Manager
Tan Kok Chong, and Kuching Radiosonde Coordinator Justin Lim Swee Hian.
Further, to the staff at the Kuching MMD station, we owe our collective
gratitude for kindly hosting us and assisting our supplemental
radiosonde launches. Our humble appreciation for the assistance,
encouragement, and patience of all of these groups and individuals
cannot be overstated. Sebastian Schmidt and Phillip Haftings (MPLNET)
and Gautier Veroone and Jerome South-ammakosane (Leosphere) were
indispensable, assisting with instrument operations in the field. NRL
and Computer Sciences Corporation participants have received financial
support from the Chief of Naval Research through the NRL Base Program
(PE 0601153N) and Office of Naval Research Codes 32 (PE 0602435N) and 35
(PE 0602114N). Author Campbell acknowledges the support of NASA
Interagency Agreement NNG13HH10I on behalf of MPLNET and the Southeast
Asia Composition, Cloud, Climate Coupling Regional Study
(SEAC4RS) Science Team (H. Maring). Financial support for
MPLNET and AERONET activities comes from the NASA Radiation Sciences
Program and SEAC4RS Science Team. Participation by Drs. Wang
and Ge for WRF modeling was supported, in part, by the NASA
Interdisciplinary Science Program.
NR 97
TC 2
Z9 2
U1 1
U2 13
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JAN
PY 2016
VL 55
IS 1
BP 3
EP 22
DI 10.1175/JAMC-D-15-0083.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DC7KE
UT WOS:000369397900001
ER
PT J
AU Raschke, E
Kinne, S
Rossow, WB
Stackhouse, PW
Wild, M
AF Raschke, Ehrhard
Kinne, Stefan
Rossow, William B.
Stackhouse, Paul W.
Wild, Martin
TI Comparison of Radiative Energy Flows in Observational Datasets and
Climate Modeling
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Aerosols; Albedo; Climatology; Cloud radiative effects; Radiation
budgets; Radiative fluxes
ID SURFACE IRRADIANCES; BUDGET PROJECT; EARTH; SATELLITE; CLOUDS; MISSION;
SYSTEM; FLUXES; TOP; PRECIPITATION
AB This study examines radiative flux distributions and local spread of values from three major observational datasets (CERES, ISCCP, and SRB) and compares them with results from climate modeling (CMIP3). Examinations of the spread and differences also differentiate among contributions from cloudy and clear-sky conditions. The spread among observational datasets is in large part caused by noncloud ancillary data. Average differences of at least 10 W m(-2) each for clear-sky downward solar, upward solar, and upward infrared fluxes at the surface demonstrate via spatial difference patterns major differences in assumptions for atmospheric aerosol, solar surface albedo and surface temperature, and/or emittance in observational datasets. At the top of the atmosphere (TOA), observational datasets are less influenced by the ancillary data errors than at the surface. Comparisons of spatial radiative flux distributions at the TOA between observations and climate modeling indicate large deficiencies in the strength and distribution of model-simulated cloud radiative effects. Differences are largest for lower-altitude clouds over low-latitude oceans. Global modeling simulates stronger cloud radiative effects (CRE) by +30 W m(-2) over trade wind cumulus regions, yet smaller CRE by about -30 W m(-2) over (smaller in area) stratocumulus regions. At the surface, climate modeling simulates on average about 15 W m(-2) smaller radiative net flux imbalances, as if climate modeling underestimates latent heat release (and precipitation). Relative to observational datasets, simulated surface net fluxes are particularly lower over oceanic trade wind regions (where global modeling tends to overestimate the radiative impact of clouds). Still, with the uncertainty in noncloud ancillary data, observational data do not establish a reliable reference.
C1 [Raschke, Ehrhard; Kinne, Stefan] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany.
[Raschke, Ehrhard] Univ Hamburg, Bundesstr 53, D-20146 Hamburg, Germany.
[Rossow, William B.] CUNY, NOAA Cooperat Remote Sensing Sci & Technol, New York, NY 10021 USA.
[Stackhouse, Paul W.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Wild, Martin] ETH, Inst Atmospher & Climate Studies, Zurich, Switzerland.
RP Raschke, E (reprint author), Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany.; Raschke, E (reprint author), Univ Hamburg, Bundesstr 53, D-20146 Hamburg, Germany.
EM ehrhard.raschke@mpimet.mpg.de
RI Wild, Martin/J-8977-2012
NR 57
TC 1
Z9 1
U1 5
U2 18
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JAN
PY 2016
VL 55
IS 1
BP 93
EP 117
DI 10.1175/JAMC-D-14-0281.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DC7KG
UT WOS:000369398100004
ER
PT J
AU Millan, L
Lebsock, M
Fishbein, E
Kalmus, P
Teixeira, J
AF Millan, Luis
Lebsock, M.
Fishbein, E.
Kalmus, P.
Teixeira, J.
TI Quantifying Marine Boundary Layer Water Vapor beneath Low Clouds with
Near-Infrared and Microwave Imagery
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Boundary layer; Microwave observations; Remote sensing; Satellite
observations
ID SEA-SURFACE TEMPERATURE; MOIST CONVECTION; ERA-INTERIM; VARIABILITY;
SENSITIVITY; CLIMATE; HEIGHT; SYSTEM; OCEANS; RETRIEVALS
AB This study investigates the synergy of collocated microwave radiometry and near-infrared imagery to estimate the marine boundary layer water vapor beneath uniform cloud fields. Microwave radiometry provides the total column water vapor, while the near-infrared imagery provides the water vapor above the cloud layers. The difference between the two gives the vapor between the surface and the cloud top, which may be interpreted as the boundary layer water vapor. In combining the two datasets, we apply several flags as well as proximity tests to remove pixels with high clouds and/or intrapixel heterogeneity. Comparisons against radiosonde and ECMWF reanalysis data demonstrate the robustness of these boundary layer water vapor estimates. Last, it is shown that the measured AMSR-MODIS boundary layer water vapor can be analyzed using sea surface temperature and cloud-top pressure information by employing simple equations based on the Clausius-Clapeyron relationship.
C1 [Millan, Luis; Lebsock, M.; Fishbein, E.; Kalmus, P.; Teixeira, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Millan, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM luis.f.millan@jpl.nasa.gov
RI Millan, Luis/J-2759-2015
FU NASA Earth Science MEaSUREs DISCOVER Project; NASA AMSR-E Science Team
FX The research described in this study was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. AMSR
data are produced by Remote Sensing Systems and sponsored by the NASA
Earth Science MEaSUREs DISCOVER Project and the NASA AMSR-E Science
Team. Data are available at www.remss.com. We are very grateful to all
the numerous participants in the field campaigns (MAGIC, VOCALS-REx,
NARVAL, and the AWI Polarstern) that made those observations possible.
NR 45
TC 0
Z9 0
U1 2
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JAN
PY 2016
VL 55
IS 1
BP 213
EP 225
DI 10.1175/JAMC-D-15-0143.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DC7KP
UT WOS:000369399100004
ER
PT J
AU Miller, KJ
Schalk, G
Hermes, D
Ojemann, JG
Rao, RPN
AF Miller, Kai J.
Schalk, Gerwin
Hermes, Dora
Ojemann, Jeffrey G.
Rao, Rajesh P. N.
TI Spontaneous Decoding of the Timing and Content of Human Object
Perception from Cortical Surface Recordings Reveals Complementary
Information in the Event-Related Potential and Broadband Spectral Change
SO PLOS COMPUTATIONAL BIOLOGY
LA English
DT Article
ID HUMAN EXTRASTRIATE CORTEX; INTRACRANIAL FIELD POTENTIALS; INFERIOR
TEMPORAL CORTEX; HUMAN VISUAL-CORTEX; PROCESSING SPEED; FUNCTIONAL MRI;
GAMMA; POWER; LOBE; REPRESENTATION
AB The link between object perception and neural activity in visual cortical areas is a problem of fundamental importance in neuroscience. Here we show that electrical potentials from the ventral temporal cortical surface in humans contain sufficient information for spontaneous and near-instantaneous identification of a subject's perceptual state. Electrocorticographic (ECoG) arrays were placed on the subtemporal cortical surface of seven epilepsy patients. Grayscale images of faces and houses were displayed rapidly in random sequence. We developed a template projection approach to decode the continuous ECoG data stream spontaneously, predicting the occurrence, timing and type of visual stimulus. In this setting, we evaluated the independent and joint use of two well-studied features of brain signals, broadband changes in the frequency power spectrum of the potential and deflections in the raw potential trace (event-related potential; ERP). Our ability to predict both the timing of stimulus onset and the type of image was best when we used a combination of both the broadband response and ERP, suggesting that they capture different and complementary aspects of the subject's perceptual state. Specifically, we were able to predict the timing and type of 96% of all stimuli, with less than 5% false positive rate and a similar to 20ms error in timing.
C1 [Miller, Kai J.] Stanford Univ, Dept Neurosurg, Stanford, CA 94305 USA.
[Miller, Kai J.] NASA, Johnson Space Ctr, Houston, TX USA.
[Miller, Kai J.; Ojemann, Jeffrey G.; Rao, Rajesh P. N.] Univ Washington, Program Neurobiol & Behav, Seattle, WA 98195 USA.
[Schalk, Gerwin] SUNY Albany, Natl Ctr Adapt Neurotechnol, Wadsworth Ctr, Dept Hlth, Albany, NY 12222 USA.
[Hermes, Dora] Stanford Univ, Psychol, Stanford, CA 94305 USA.
[Ojemann, Jeffrey G.] Univ Washington, Dept Neurol Surg, Seattle, WA USA.
[Ojemann, Jeffrey G.; Rao, Rajesh P. N.] Univ Washington, Ctr Sensorimotor Neural Engn, Seattle, WA 98195 USA.
[Rao, Rajesh P. N.] Univ Washington, Comp Sci & Engn, Seattle, WA 98195 USA.
RP Miller, KJ (reprint author), Stanford Univ, Dept Neurosurg, Stanford, CA 94305 USA.; Miller, KJ (reprint author), NASA, Johnson Space Ctr, Houston, TX USA.; Miller, KJ (reprint author), Univ Washington, Program Neurobiol & Behav, Seattle, WA 98195 USA.
EM kai.miller@stanford.edu
OI Ojemann, Jeffrey/0000-0001-7580-8934
FU National Aeronautics and Space Administration Graduate Student Research
Program; NIH [R01-NS065186, T32-EY20485, R01-EB00856, P41-EB018783]; NSF
[EEC-1028725]; US Army Research Office [W911NF-14-1-0440]
FX This work was supported by National Aeronautics and Space Administration
Graduate Student Research Program (KJM), the NIH (R01-NS065186 (KJM,
JGO, RPNR), T32-EY20485 (DH), R01-EB00856 (GS) and P41-EB018783 (GS)),
the NSF (EEC-1028725 (RPNR)), and the US Army Research Office
(W911NF-14-1-0440 (GS)). The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 57
TC 1
Z9 1
U1 1
U2 4
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1553-734X
EI 1553-7358
J9 PLOS COMPUT BIOL
JI PLoS Comput. Biol.
PD JAN
PY 2016
VL 12
IS 1
AR e1004660
DI 10.1371/journal.pcbi.1004660
PG 20
WC Biochemical Research Methods; Mathematical & Computational Biology
SC Biochemistry & Molecular Biology; Mathematical & Computational Biology
GA DC6YS
UT WOS:000369366100012
PM 26820899
ER
PT J
AU Bryan, S
Ade, P
Amiri, M
Benton, S
Bihary, R
Bock, J
Bond, JR
Chiang, HC
Contaldi, C
Crill, B
Dore, O
Elder, B
Filippini, J
Fraisse, A
Gambrel, A
Gandilo, N
Gudmundsson, J
Hasselfield, M
Halpern, M
Hilton, G
Holmes, W
Hristov, V
Irwin, K
Jones, W
Kermish, Z
Lawrie, C
MacTavish, C
Mason, P
Megerian, K
Moncelsi, L
Montroy, T
Morford, T
Nagy, J
Netterfield, CB
Padilla, I
Rahlin, AS
Reintsema, C
Riley, DC
Ruhl, J
Runyan, M
Saliwanchik, B
Shariff, J
Soler, J
Trangsrud, A
Tucker, C
Tucker, R
Turner, A
Wen, S
Wiebe, D
Young, E
AF Bryan, Sean
Ade, Peter
Amiri, Mandana
Benton, Steven
Bihary, Richard
Bock, James
Bond, J. Richard
Chiang, H. Cynthia
Contaldi, Carlo
Crill, Brendan
Dore, Olivier
Elder, Benjamin
Filippini, Jeffrey
Fraisse, Aurelien
Gambrel, Anne
Gandilo, Natalie
Gudmundsson, Jon
Hasselfield, Matthew
Halpern, Mark
Hilton, Gene
Holmes, Warren
Hristov, Viktor
Irwin, Kent
Jones, William
Kermish, Zigmund
Lawrie, Craig
MacTavish, Carrie
Mason, Peter
Megerian, Krikor
Moncelsi, Lorenzo
Montroy, Thomas
Morford, Tracy
Nagy, Johanna
Netterfield, C. Barth
Padilla, Ivan
Rahlin, Alexandra S.
Reintsema, Carl
Riley, Daniel C.
Ruhl, John
Runyan, Marcus
Saliwanchik, Benjamin
Shariff, Jamil
Soler, Juan
Trangsrud, Amy
Tucker, Carole
Tucker, Rebecca
Turner, Anthony
Wen, Shyang
Wiebe, Donald
Young, Edward
TI A cryogenic rotation stage with a large clear aperture for the half-wave
plates in the Spider instrument
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID POLARIMETRY; POLARIZATION; SYSTEMATICS
AB We describe the cryogenic half-wave plate rotation mechanisms built for and used in SPIDER., a polarization-sensitive balloon-borne telescope array that observed the cosmic microwave background at 95 GHz and 150 GHz during a stratospheric balloon flight from Antarctica in January 2015. The mechanisms operate at liquid helium temperature in flight. A three-point contact design keeps the mechanical bearings relatively small but allows for a large (305 mm) diameter clear aperture. A worm gear driven by a cryogenic stepper motor allows for precise positioning and prevents undesired rotation when the motors are depowered. A custom-built optical encoder system monitors the bearing angle to an absolute accuracy of +/-0.1 degrees. The system performed well in SPIDER. during its successful 16 day flight. (C) 2016 AIP Publishing LLC.
C1 [Bryan, Sean] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Ade, Peter; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Amiri, Mandana; Halpern, Mark; Wiebe, Donald] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Benton, Steven; Fraisse, Aurelien; Gambrel, Anne; Gudmundsson, Jon; Jones, William; Kermish, Zigmund; Rahlin, Alexandra S.; Young, Edward] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Benton, Steven; Netterfield, C. Barth; Padilla, Ivan; Shariff, Jamil] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Bihary, Richard; Elder, Benjamin; Lawrie, Craig; Montroy, Thomas; Nagy, Johanna; Riley, Daniel C.; Ruhl, John; Saliwanchik, Benjamin; Shariff, Jamil; Wen, Shyang] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Bihary, Richard; Elder, Benjamin; Lawrie, Craig; Montroy, Thomas; Nagy, Johanna; Riley, Daniel C.; Ruhl, John; Saliwanchik, Benjamin; Shariff, Jamil; Wen, Shyang] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Bock, James; Crill, Brendan; Dore, Olivier; Hristov, Viktor; Mason, Peter; Moncelsi, Lorenzo; Morford, Tracy; Trangsrud, Amy; Tucker, Rebecca] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Bock, James; Crill, Brendan; Dore, Olivier; Holmes, Warren; Megerian, Krikor; Runyan, Marcus; Trangsrud, Amy; Turner, Anthony] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bond, J. Richard] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Chiang, H. Cynthia] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa.
[Contaldi, Carlo] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Theoret Phys, London, England.
[Filippini, Jeffrey] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Gandilo, Natalie; Netterfield, C. Barth] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
[Hasselfield, Matthew] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hilton, Gene; Reintsema, Carl] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Irwin, Kent] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[MacTavish, Carrie] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England.
[Netterfield, C. Barth] CIFAR Program Cosmol & Grav, Canadian Inst Adv Res, Toronto, ON M5S 3H8, Canada.
[Soler, Juan] Inst Astrophys Spatiale, Orsay, France.
RP Bryan, S (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM sean.a.bryan@asu.edu
FU U.S. by National Aeronautics and Space Administration through Science
Mission Directorate [NNX07AL64G, NNX12AE95G]; NESSF [NNX10AM55H];
National Science Foundation [PLR-1043515]; David and Lucile Packard
Foundation; National Sciences and Engineering Council; Canadian Space
Agency
FX SPIDER is supported in the U.S. by National Aeronautics and Space
Administration under Grant Nos. NNX07AL64G and NNX12AE95G issued through
the Science Mission Directorate, with support for A.S.R. from NESSF
NNX10AM55H, and by the National Science Foundation through No.
PLR-1043515. Logistical support for the Antarctic deployment and
operations was provided by the NSF through the U.S. Antarctic Program.
The collaboration is grateful for the generous support of the David and
Lucile Packard Foundation, which has been crucial to the success of the
project.; Support in Canada is provided by the National Sciences and
Engineering Council and the Canadian Space Agency.
NR 24
TC 1
Z9 1
U1 1
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD JAN
PY 2016
VL 87
IS 1
AR 014501
DI 10.1063/1.4939435
PG 9
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA DC7WH
UT WOS:000369430900033
PM 26827333
ER
PT J
AU Isac, A
Mandea, M
Purucker, M
Langlais, B
AF Isac, Anca
Mandea, Mioara
Purucker, Michael
Langlais, Benoit
TI A comparative analysis of the magnetic field signals over impact
structures on the Earth, Mars and the Moon
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Terrestrial planets; Impact craters; Magnetic characteristics
ID MARTIAN CRUST; MAGSAT DATA; DEMAGNETIZATION; ANOMALIES; EVOLUTION;
MODEL; SHOCK; TOPOGRAPHY; PYRRHOTITE; CRATERS
AB An improved description of magnetic fields of terrestrial bodies has been obtained from recent space missions, leading to a better characterization of the internal fields including those of crustal origin. One of the striking differences in their crustal magnetic field is the signature of large impact craters. A comparative analysis of the magnetic characteristics of these structures can shed light on the history of their respective planetary-scale magnetic dynamos. This has motivated us to identify impact craters and basins, first by their quasi-circular features from the most recent and detailed topographic maps and then from available global magnetic field maps. We have examined the magnetic field observed above 27 complex craters on the Earth, 34 impact basins on Mars and 37 impact basins on the Moon. For the first time, systematic trends in the amplitude and frequency of the magnetic patterns, inside and outside of these structures are observed for all three bodies. The demagnetization effects due to the impact shock wave and excavation processes have been evaluated applying the Equivalent Source Dipole forward modeling approach. The main characteristics of the selected impact craters are shown. The trends in their magnetic signatures are indicated, which are related to the presence or absence of a planetary-scale dynamo at the time of their formation and to impact processes.
The low magnetic field intensity at center can be accepted as the prime characteristic of a hypervelocity impact and strongly associated with the mechanics of impact crater formation. In the presence of an active internal field, the process of demagnetization due to the shock impact is associated with post-impact remagnetization processes, generating a more complex magnetic signature. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Isac, Anca] Geol Inst Romania, 1 Caransebes Str, RO-012271 Bucharest, Romania.
[Mandea, Mioara] CNES, 2 Pl Maurice Quentin, F-75039 Paris 01, France.
[Purucker, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Langlais, Benoit] CNRS, UMR 6112, Lab Planetol & Geodynam Nantes, Nantes, France.
[Langlais, Benoit] Univ Nantes, Nantes, France.
RP Isac, A (reprint author), Geol Inst Romania, 1 Caransebes Str, RO-012271 Bucharest, Romania.
EM anca.isac@igr.ro; mioara.mandea@cnes.fr; michael.e.purucker@nasa.gov;
benoit.langlais@univ-nantes.fr
RI MANDEA, Mioara/E-4892-2012
NR 68
TC 0
Z9 0
U1 1
U2 6
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 1
PY 2016
VL 57
IS 1
BP 477
EP 492
DI 10.1016/j.asr.2015.11.019
PG 16
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DB5OU
UT WOS:000368564300038
ER
PT J
AU Ackermann, M
Ajello, M
Atwood, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Gonzalez, JB
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bonino, R
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caputo, R
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Cohen, JM
Cohen-Tanugi, J
Cominsky, LR
Conrad, J
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Di Mauro, M
Di Venere, L
Dominguez, A
Drell, PS
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Franckowiak, A
Fukazawa, Y
Funk, S
Furniss, AK
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Guillemot, L
Guiriec, S
Harding, AK
Hays, E
Hewitt, JW
Hill, AB
Horan, D
Iafrate, G
Hartmann, D
Jogler, T
Johannesson, G
Johnson, AS
Kamae, T
Kataoka, J
Knodlseder, J
Kuss, M
La Mura, G
Larsson, S
Latronico, L
Lemoine-Goumard, M
Li, J
Li, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Michelson, PF
Mirabal, N
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nuss, E
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Petrosian, V
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Romani, RW
Sanchez-Conde, M
Parkinson, PMS
Schmid, J
Schulz, A
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Suson, DJ
Tajima, H
Takahashi, H
Takahashi, M
Takahashi, T
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Vianello, G
Wood, KS
Wood, M
Yassine, M
Zaharijas, G
Zimmer, S
AF Ackermann, M.
Ajello, M.
Atwood, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Gonzalez, J. Becerra
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caputo, R.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Cohen, J. M.
Cohen-Tanugi, J.
Cominsky, L. R.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Di Mauro, M.
Di Venere, L.
Dominguez, A.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Furniss, A. K.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Guillemot, L.
Guiriec, S.
Harding, A. K.
Hays, E.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Iafrate, G.
Hartmann, Dieter
Jogler, T.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
La Mura, G.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mirabal, N.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Petrosian, V.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Romani, R. W.
Sanchez-Conde, M.
Parkinson, P. M. Saz
Schmid, J.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Suson, D. J.
Tajima, H.
Takahashi, H.
Takahashi, M.
Takahashi, T.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Wood, K. S.
Wood, M.
Yassine, M.
Zaharijas, G.
Zimmer, S.
TI 2FHL: THE SECOND CATALOG OF HARD FERMI-LAT SOURCES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-rays: general
ID LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; GAMMA-RAY
EMISSION; GALAXY SURVEY DATA; ENERGETIC PSR J1357-6429; REMNANT RCW 86;
MULTIWAVELENGTH OBSERVATIONS; SUPERNOVA-REMNANTS; SKY SURVEY; HESS
AB We present a catalog of sources detected above 50 GeV by the Fermi-Large Area Telescope (LAT) in 80 months of data. The newly delivered Pass. 8 event-level analysis allows the detection and characterization of sources in the 50 GeV-2 TeV energy range. In this energy band, Fermi-LAT. has detected 360 sources, which constitute the second catalog of hard Fermi-LAT. sources (2FHL). The improved angular resolution enables the precise localization of point sources (similar to 1.' 7 radius at 68% C.L.) and the detection and characterization of spatially extended sources. We find that 86% of the sources can be associated with counterparts at other wavelengths, of which the majority (75%) are active galactic nuclei and the rest (11%) are Galactic sources. Only 25% of the 2FHL sources have been previously detected by Cherenkov telescopes, implying that the 2FHL provides a reservoir of candidates to be followed up at very high energies. This work closes the energy gap between the observations performed at GeV energies by Fermi-LAT. on orbit and the observations performed at higher energies by Cherenkov telescopes from the ground.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Dominguez, A.; Hartmann, Dieter] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Atwood, W. B.; Caputo, R.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Caputo, R.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Furniss, A. K.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tajima, H.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Furniss, A. K.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tajima, H.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ballet, J.; Grenier, I. A.; Schmid, J.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Gonzalez, J. Becerra; Brandt, T. J.; Buson, S.; Cohen, J. M.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Mirabal, N.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra; Cohen, J. M.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra; Cohen, J. M.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Cuoco, A.; Desiante, R.; Latronico, L.; Maldera, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Yassine, M.] Univ Montpellier, CNRS, IN2P3, Lab Univ & Particules Montpellier, F-34059 Montpellier, France.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Buson, S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Buson, S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Buson, S.; Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA.
[Buson, S.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Caliandro, G. A.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Cheung, C. C.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Conrad, J.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.] INAF, Osservatorio Astron Roma, I-00040 Rome, Italy.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Fortin, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Grondin, M. -H.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Guillemot, L.] Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France.
[Guillemot, L.] CNRS, INSU, Stn Radioastron Nancay Observ Paris, F-18330 Nancay, France.
[Hewitt, J. W.] Univ N Florida, Dept Phys, Jacksonville, FL 32224 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France.
[La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[La Mura, G.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, E-08193 Barcelona, Spain.
[Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.; Takahashi, M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain.
[Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, SI-5000 Nova Gorica, Slovenia.
RP Gasparrini, D (reprint author), Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
EM jcohen@astro.umd.edu; gasparrini@asdc.asi.it
RI Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; giglietto,
nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Bissaldi,
Elisabetta/K-7911-2016; Orlando, E/R-5594-2016; Funk,
Stefan/B-7629-2015; Bonino, Raffaella/S-2367-2016; Torres,
Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017;
OI Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385;
giglietto, nicola/0000-0002-9021-2888; Moskalenko,
Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106;
Funk, Stefan/0000-0002-2012-0080; Torres, Diego/0000-0002-1522-9065; Di
Venere, Leonardo/0000-0003-0703-824X; Sgro',
Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791;
Gargano, Fabio/0000-0002-5055-6395; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Hill, Adam/0000-0003-3470-4834; Dominguez,
Alberto/0000-0002-3433-4610; orienti, monica/0000-0003-4470-7094; DI
MAURO, MATTIA/0000-0003-2759-5625; Cutini, Sara/0000-0002-1271-2924;
Becerra Gonzalez, Josefa/0000-0002-6729-9022
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique/Institut National de Physique Nucleaire 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; 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 d' Etudes Spatiales in France
FX 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 a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire 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 d' Etudes Spatiales in France. 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 research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France.
NR 87
TC 32
Z9 32
U1 3
U2 7
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 JAN
PY 2016
VL 222
IS 1
AR 5
DI 10.3847/0067-0049/222/1/5
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC1NF
UT WOS:000368982300005
ER
PT J
AU Liu, T
Zhang, QZ
Kim, KT
Wu, YF
Lee, CW
Lee, JE
Tatematsu, K
Choi, M
Juvela, M
Thompson, M
Goldsmith, PF
Liu, SY
Naomi, H
Koch, P
Henkel, C
Sanhueza, P
He, JH
Rivera-Ingraham, A
Wang, K
Cunningham, MR
Tang, YW
Lai, SP
Yuan, JH
Li, D
Fuller, G
Kang, MJ
Luong, QN
Liu, HB
Ristorcelli, I
Yang, J
Xu, Y
Hirota, T
Mardones, D
Qin, SL
Chen, HR
Kwon, W
Meng, FY
Zhang, HW
Kim, MR
Yi, HW
AF Liu, Tie
Zhang, Qizhou
Kim, Kee-Tae
Wu, Yuefang
Lee, Chang Won
Lee, Jeong-Eun
Tatematsu, Ken'ichi
Choi, Minho
Juvela, Mika
Thompson, Mark
Goldsmith, Paul F.
Liu, Sheng-yuan
Naomi, Hirano
Koch, Patrick
Henkel, Christian
Sanhueza, Patricio
He, JinHua
Rivera-Ingraham, Alana
Wang, Ke
Cunningham, Maria R.
Tang, Ya-Wen
Lai, Shih-Ping
Yuan, Jinghua
Li, Di
Fuller, Gary
Kang, Miju
Luong, Quang Nguyen
Liu, Hauyu Baobab
Ristorcelli, Isabelle
Yang, Ji
Xu, Ye
Hirota, Tomoya
Mardones, Diego
Qin, Sheng-Li
Chen, Huei-Ru
Kwon, Woojin
Meng, Fanyi
Zhang, Huawei
Kim, Mi-Ryang
Yi, Hee-Weon
TI PLANCK COLD CLUMPS IN THE lambda ORIONIS COMPLEX. I. DISCOVERY OF AN
EXTREMELY YOUNG CLASS 0 PROTOSTELLAR OBJECT AND A PROTO-BROWN DWARF
CANDIDATE IN THE BRIGHT-RIMMED CLUMP PGCC G192.32-11.88
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: jets and outflows; ISM: kinematics and dynamics; stars: formation
ID MASSIVE-STAR-FORMATION; SPECTRAL ENERGY-DISTRIBUTIONS; RADIATION-DRIVEN
IMPLOSION; IRAS POINT SOURCES; H-II REGIONS; STELLAR OBJECTS; MOLECULAR
CLOUDS; SUBMILLIMETER ARRAY; FORMING REGION; CORES
AB We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the lambda Orionis complex in order to systematically investigate the effects of stellar feedback. In the particular case of PGCC G192.32-11.88, we discovered an extremely young Class 0 protostellar object (G192N) and a proto-brown dwarf candidate (G192S). G192N and G192S are located in a gravitationally bound brightrimmed clump. The velocity and temperature gradients seen in line emission of CO isotopologues indicate that PGCC G192.32-11.88 is externally heated and compressed. G192N probably has the lowest bolometric luminosity (similar to 0.8 L-circle dot) and accretion rate (6.3 x 10(-7) M-circle dot yr(-1)) when compared with other young Class 0 sources (e.g., PACS Bright Red Sources) in the Orion complex. It has slightly larger internal luminosity (0.21 +/- 0.01 L-circle dot) and outflow velocity (similar to 14 km s(-1)) than the predictions of first hydrostatic cores (FHSCs). G192N might be among the youngest Class 0 sources, which are slightly more evolved than an FHSC. Considering its low internal luminosity (0.08 +/- 0.01 L-circle dot) and accretion rate (2.8 x 10(-8) M-circle dot yr(-1)), G192S is an ideal proto-brown dwarf candidate. The star formation efficiency (similar to 0.3%-0.4%) and core formation efficiency (similar to 1%) in PGCC G192.32-11.88 are significantly smaller than in other giant molecular clouds or filaments, indicating that the star formation therein is greatly suppressed owing to stellar feedback.
C1 [Liu, Tie; Kim, Kee-Tae; Lee, Chang Won; Choi, Minho; Kang, Miju; Kwon, Woojin; Kim, Mi-Ryang] Korea Astron & Space Sci Inst, Daejeon 34055, South Korea.
[Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wu, Yuefang; Zhang, Huawei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Lee, Chang Won] Univ Sci & Technol, Daejeon 305333, South Korea.
[Lee, Jeong-Eun; Yi, Hee-Weon] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea.
[Tatematsu, Ken'ichi; Sanhueza, Patricio; Luong, Quang Nguyen; Hirota, Tomoya] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Juvela, Mika] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland.
[Thompson, Mark] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liu, Sheng-yuan; Naomi, Hirano; Koch, Patrick; Tang, Ya-Wen; Liu, Hauyu Baobab; Chen, Huei-Ru] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Henkel, Christian] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Henkel, Christian] Abdulaziz Univ, Dept Astron, Jeddah 21589, Saudi Arabia.
[He, JinHua] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Yunnan Observ, Kunming 650011, Yunnan Province, Peoples R China.
[Rivera-Ingraham, Alana] ESA ESAC, E-28691 Madrid, Spain.
[Wang, Ke] European So Observ, D-85748 Garching, Germany.
[Cunningham, Maria R.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan.
[Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan.
[Yuan, Jinghua; Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Li, Di] Chinese Acad Sci, Key Lab Radio Astron, Beijing 100864, Peoples R China.
[Fuller, Gary] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ristorcelli, Isabelle] Univ Toulouse 3, CNRS, IRAP, UMR5277, F-31028 Toulouse 4, France.
[Yang, Ji; Xu, Ye] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China.
[Mardones, Diego] Univ Chile, Dept Astron, Santiago, Chile.
[Qin, Sheng-Li] Yunnan Univ, Dept Astron, Kunming 650091, Peoples R China.
[Qin, Sheng-Li] Yunnan Univ, Key Lab Astroparticle Phys Yunnan Prov, Kunming 650091, Peoples R China.
[Meng, Fanyi] Univ Cologne, Inst Phys, D-50937 Cologne, Germany.
RP Liu, T (reprint author), Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea.
EM liutiepku@gmail.com
RI Goldsmith, Paul/H-3159-2016; Mardones, Diego/I-5719-2016
FU KASI fellowship; China Ministry of Science and Technology under State
Key Development Program for Basic Research [2012CB821800]; NSFC
[11373009, 11433008]; ESO fellowship; DFG Priority Program ("Physics of
the Interstellar Medium") [1573, WA3628-1/1]; National Research
Foundation of Korea (NRF) - Ministry of Education, Science, and
Technology [NRF-2013R1A1A2A10005125]; global research collaboration of
the Korea Research Council of Fundamental Science & Technology (KRCF);
National Research Foundation of Korea (NRF) [NRF-2015R1A2A2A01004769];
Korea Astronomy and Space Science Institute under the RD program
[2015-1-320-18]; Ministry of Science and Technology of Taiwan [MoST
102-2119-M-007-004-MY3]
FX We are grateful to the SMA, PMO, CSO, JCMT, and the KVN staff. T.L. is
supported by KASI fellowship. Y.W. is partly supported by the China
Ministry of Science and Technology under State Key Development Program
for Basic Research (No. 2012CB821800), the grants of NSFC No. 11373009
and No. 11433008. K. W. acknowledges the support from the ESO fellowship
and DFG Priority Program 1573 ("Physics of the Interstellar Medium")
grant WA3628-1/1. C.W.L. was supported by the Basic Science Research
Program through the National Research Foundation of Korea (NRF) funded
by the Ministry of Education, Science, and Technology
(NRF-2013R1A1A2A10005125) and also by the global research collaboration
of the Korea Research Council of Fundamental Science & Technology
(KRCF). This work was carried out in part at the Jet Propulsion
Laboratory, operated for NASA by the California Institute of Technology.
J.-E.L. was supported by the Basic Science Research Program through the
National Research Foundation of Korea (NRF) (grant No.
NRF-2015R1A2A2A01004769) and the Korea Astronomy and Space Science
Institute under the R&D program (Project No. 2015-1-320-18) supervised
by the Ministry of Science, ICT, and Future Planning. The KVN is a
facility operated by the Korea Astronomy and Space Science Institute.
S.P.L. thanks the support of the Ministry of Science and Technology of
Taiwan with grant MoST 102-2119-M-007-004-MY3. Figures 24 and 25 are
used with permission from Dr. A. Stutz.
NR 104
TC 3
Z9 3
U1 1
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 JAN
PY 2016
VL 222
IS 1
AR 7
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC1NF
UT WOS:000368982300007
ER
PT J
AU Sabbi, E
Lennon, DJ
Anderson, J
Cignoni, M
van der Marel, RP
Zaritsky, D
De Marchi, G
Panagia, N
Gouliermis, DA
Grebel, EK
Gallagher, JS
Smith, LJ
Sana, H
Aloisi, A
Tosi, M
Evans, CJ
Arab, H
Boyer, M
de Mink, SE
Gordon, K
Koekemoer, AM
Larsen, SS
Ryon, JE
Zeidler, P
AF Sabbi, E.
Lennon, D. J.
Anderson, J.
Cignoni, M.
van der Marel, R. P.
Zaritsky, D.
De Marchi, G.
Panagia, N.
Gouliermis, D. A.
Grebel, E. K.
Gallagher, J. S., III
Smith, L. J.
Sana, H.
Aloisi, A.
Tosi, M.
Evans, C. J.
Arab, H.
Boyer, M.
de Mink, S. E.
Gordon, K.
Koekemoer, A. M.
Larsen, S. S.
Ryon, J. E.
Zeidler, P.
TI HUBBLE TARANTULA TREASURY PROJECT. III. PHOTOMETRIC CATALOG AND
RESULTING CONSTRAINTS ON THE PROGRESSION OF STAR FORMATION IN THE 30
DORADUS REGION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: star clusters: individual (30 Doradus); Magellanic
Clouds; stars: formation; stars: imaging; stars: pre-main sequence
ID LARGE-MAGELLANIC-CLOUD; INITIAL MASS FUNCTION; GRAVITATIONAL LENSING
EXPERIMENT; SUPERNOVA REMNANT N157B; GALAXY EVOLUTION SAGE; ALL-SKY
SURVEY; M-CIRCLE-DOT; SPACE-TELESCOPE; LUMINOSITY FUNCTION;
INTERSTELLAR-MEDIUM
AB We present and describe the astro-photometric catalog of more than 800,000 sources found in the Hubble Tarantula Treasury Project (HTTP). HTTP is a Hubble Space Telescope Treasury program designed to image the entire 30 Doradus region down to the sub-solar (similar to 0.5M(circle dot)) mass regime using the Wide Field Camera 3 and the Advanced Camera for Surveys. We observed 30 Doradus in the near-ultraviolet (F275W, F336W), optical (F555W, F658N, F775W), and near-infrared (F110W, F160W) wavelengths. The stellar photometry was measured using point-spread function fitting across all. bands simultaneously. The relative astrometric accuracy of the catalog is 0.4 mas. The astro-photometric catalog, results from artificial star experiments, and the mosaics for all the filters are available for download. Color-magnitude diagrams are presented showing the spatial distributions and ages of stars within 30 Dor as well as in the surrounding fields. HTTP provides the first rich and statistically significant sample of intermediate-and low-mass pre-main sequence candidates and allows us to trace how star formation has been developing through the region. The depth and high spatial resolution of our analysis highlight the dual role of stellar feedback in quenching and triggering star formation on the giant H II region scale. Our results are consistent with stellar sub-clustering in a partially filled gaseous nebula that is offset toward our side of the Large Magellanic Cloud.
C1 [Sabbi, E.; Anderson, J.; Cignoni, M.; van der Marel, R. P.; Panagia, N.; Sana, H.; Aloisi, A.; Arab, H.; Gordon, K.; Koekemoer, A. M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Lennon, D. J.] ESA European Space Astron Ctr, Apdo Correo 78, E-28691 Madrid, Spain.
[Zaritsky, D.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[De Marchi, G.] European Space Agcy, Dept Space Sci, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands.
[Panagia, N.] Osserv Astrofis Catania, Ist Nazl Astrofis, Via Santa Sofia 78, I-95123 Catania, Italy.
[Panagia, N.] Supernova Ltd, OYV 131,Northsound Rd, Virgin Gorda, British Virgin, England.
[Gouliermis, D. A.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
[Gouliermis, D. A.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Grebel, E. K.; Zeidler, P.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Gallagher, J. S., III; Ryon, J. E.] Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA.
[Smith, L. J.] ESA STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Tosi, M.] Osservatorio Astron Bologna, Ist Nazl Astrofis, Via Ranzani 1, I-40127 Bologna, Italy.
[Evans, C. J.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Boyer, M.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[de Mink, S. E.] Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands.
[Larsen, S. S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
RP Sabbi, E (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM sabbi@stsci.edu
RI Cignoni, Michele/J-9365-2016; Tosi, Monica/O-9377-2015; Sana,
Hugues/B-2664-2013;
OI Cignoni, Michele/0000-0001-6291-6813; Tosi, Monica/0000-0002-0986-4759;
Sana, Hugues/0000-0001-6656-4130; de Mink, Selma/0000-0001-9336-2825;
Lennon, Daniel/0000-0003-3063-4867; /0000-0002-1891-3794; Koekemoer,
Anton/0000-0002-6610-2048
FU NASA [NAS 5-26555]; NASA through grants from the Space Telescope Science
Institute [12499, 12939]; German Research Foundation (DFG) [GO 1659/3-2,
SFB 881, B5]; European Commission [H2020-MSCA-IF-2014, 661502]; Italian
MIUR [PRIN-MIUR 2010LY5N2T]
FX We thank the anonymous referee for the thorough review and highly
appreciate the comments and suggestions. which significantly contributed
to improving the quality of this paper. We thank Karen Levay and the
MAST HLSP Team at STScI for their invaluable help in releasing to the
astronomical community all the high level science products associated
with HTTP. Based on observations with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute, which is
operated by AURA Inc., under NASA contract NAS 5-26555. These
observations were associated with Programs 12499 and 12939. Support for
both Programs 12499 and 12939 was provided by NASA through grants from
the Space Telescope Science Institute. D.A.G. kindly acknowledges
financial support by the German Research Foundation (DFG) through grant
GO 1659/3-2. S.d.M. acknowledges support by the European Commission,
grant H2020-MSCA-IF-2014, project ID 661502. M.T. was partially funded
by the Italian MIUR through the grant PRIN-MIUR 2010LY5N2T. E.K.G.
acknowledges support by Sonderforschungsbereich SFB 881 "The Milky Way
System" of the German Research Foundation (DFG), particularly subproject
B5.
NR 94
TC 4
Z9 4
U1 2
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 JAN
PY 2016
VL 222
IS 1
AR 11
DI 10.3847/0067-0049/222/1/11
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC1NF
UT WOS:000368982300011
ER
PT J
AU Munia, H
Guillaume, JHA
Mirumachi, N
Porkka, M
Wada, Y
Kummu, M
AF Munia, H.
Guillaume, J. H. A.
Mirumachi, N.
Porkka, M.
Wada, Y.
Kummu, M.
TI Water stress in global transboundary river basins: significance of
upstream water use on downstream stress
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE transboundary river basins; upstream water use; water stress;
upstream-downstream relations; sub-basin; conflict; cooperation
ID ENVIRONMENTAL FLOW REQUIREMENTS; CLIMATE-CHANGE; SPATIALLY EXPLICIT;
CONFLICT; COOPERATION; DEMAND; VARIABILITY; WITHDRAWALS; RESOURCES;
SCARCITY
AB Growing population and water demand have increased pressure on water resources in various parts of the globe, including many transboundary river basins. While the impacts of upstream water use on downstream water availability have been analysed in many of these international river basins, this has not been systematically done at the global scale using coherent and comparable datasets. In this study, we aim to assess the change in downstream water stress due to upstream water use in the world's transboundary river basins. Water stress was first calculated considering only local water use of each sub-basin based on country-basin mesh, then compared with the situation when upstream water use was subtracted from downstream water availability. We found that water stress was generally already high when considering only local water use, affecting 0.95-1.44 billion people or 33%-51% of the population in transboundary river basins. After accounting for upstream water use, stress level increased by at least 1 percentage-point for 30-65 sub-basins, affecting 0.29-1.13 billion people. Altogether 288 out of 298 middle-stream and downstream sub-basin areas experienced some change in stress level. Further, we assessed whether there is a link between increased water stress due to upstream water use and the number of conflictive and cooperative events in the transboundary river basins, as captured by two prominent databases. No direct relationship was found. This supports the argument that conflicts and cooperation events originate from a combination of different drivers, among which upstream-induced water stress may play a role. Our findings contribute to better understanding of upstream-downstream dynamics in water stress to help address water allocation problems.
C1 [Munia, H.; Guillaume, J. H. A.; Porkka, M.; Kummu, M.] Aalto Univ, Water & Dev Res Grp, Tietotie 1E, FI-02150 Espoo, Finland.
[Mirumachi, N.] Kings Coll London, Dept Geog, London WC2R 2LS, England.
[Wada, Y.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Wada, Y.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
[Wada, Y.] Univ Utrecht, Fac Geosci, Dept Phys Geog, Heidelberglaan 2, NL-3584 CS Utrecht, Netherlands.
RP Munia, H (reprint author), Aalto Univ, Water & Dev Res Grp, Tietotie 1E, FI-02150 Espoo, Finland.
EM hafsa.munia@aalto.fi
RI Kummu, Matti/C-4797-2011; Porkka, Miina/M-6106-2014
OI Kummu, Matti/0000-0001-5096-0163; Porkka, Miina/0000-0002-8285-6122
FU Academy of Finland [269901, 267463]; Japan Society for the Promotion of
Science (JSPS) Overseas Research Fellowship [JSPS-2014-878]; Maa- ja
vesitekniikan tuki ry
FX This work was funded by Maa- ja vesitekniikan tuki ry. Joseph Guillaume
received funding from Academy of Finland funded project NexusAsia (grant
no. 269901). Yoshihide Wada is supported by Japan Society for the
Promotion of Science (JSPS) Overseas Research Fellowship
(JSPS-2014-878). Matti Kummu received funding from Academy of Finland
funded project SCART (grant no. 267463).
NR 48
TC 2
Z9 2
U1 3
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD JAN
PY 2016
VL 11
IS 1
AR 014002
DI 10.1088/1748-9326/11/1/014002
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DB8YT
UT WOS:000368803800005
ER
PT J
AU Rodgveller, CJ
Stark, JW
Echave, KB
Hulson, PJF
AF Rodgveller, Cara J.
Stark, James W.
Echave, Katy B.
Hulson, Peter-John F.
TI Age at maturity, skipped spawning, and fecundity of female sablefish
(Anoplopoma fimbria) during the spawning season
SO FISHERY BULLETIN
LA English
DT Article
ID COD GADUS-MORHUA; DATA-STORAGE TAGS; ATLANTIC COD; REFERENCE POINTS;
MATERNAL AGE; GROWTH; FISHERIES; WATERS; ALASKA; REPRODUCTION
AB Accurate maturity-at-age data are necessary for estimating spawning stock biomass and setting reference points for fishing. This study is the first on age at maturity of female sablefish (Anoplopoma fimbria) sampled in Alaska during their winter spawning period, when maturity is most easily assessed. Skipped spawning, the situation where fish that have spawned in the past do not spawn during the current season, was documented in female sablefish for the first time. Determination of age at maturity was heavily influenced by whether these fish that would skip spawning were classified as mature or immature; age at 50% maturity was 6.8 years when fish that would skip spawning were classified as mature, and 9.9 years when classified as immature. Skipped spawning was more common on the continental shelf, and rates of skipped spawning increased with age through age 15. Estimates of age at maturity were similar for samples collected in winter and summer, when fish that would skip spawning sampled during winter were classified as mature. When fish that would skip spawning were considered immature in the sable fish population model for Alaska, estimates of spawning biomass decreased. Relative fecundity did not change with size and age, verifying the assumption made in the Alaska sablefish stock assessment that relative reproductive output is linearly related to female spawning biomass.
C1 [Rodgveller, Cara J.; Stark, James W.; Echave, Katy B.; Hulson, Peter-John F.] NOAA, Alaska Biol Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
RP Rodgveller, CJ (reprint author), NOAA, Alaska Biol Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM cara.rodgveller@noaa.gov
NR 33
TC 1
Z9 1
U1 6
U2 12
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD JAN
PY 2016
VL 114
IS 1
BP 89
EP 102
DI 10.7755/FB.114.1.8
PG 14
WC Fisheries
SC Fisheries
GA DC2LF
UT WOS:000369047500008
ER
PT J
AU Aydemir, U
Zevalkink, A
Ormeci, A
Bux, S
Snyder, GJ
AF Aydemir, Umut
Zevalkink, Alex
Ormeci, Alim
Bux, Sabah
Snyder, G. Jeffrey
TI Enhanced thermoelectric properties of the Zintl phase BaGa2Sb2 via
doping with Na or K
SO JOURNAL OF MATERIALS CHEMISTRY A
LA English
DT Article
ID ELECTRON LOCALIZATION FUNCTION; INTERMETALLIC COMPOUNDS;
POWER-GENERATION; EFFICIENCY; COMPOUND; REPRESENTATION; SKUTTERUDITES;
CLATHRATE; FRAMEWORK; SUBSTITUTION
AB Na- or K-doped samples of Ba1-x(Na, K)(x)Ga2Sb2 were prepared by ball-milling followed by hot-pressing. The topological analysis of the electron density of BaGa2Sb2 implies a polar covalent nature of the Sb-Ga bonds in which the Sb atoms receive the electrons transferred from Ba rather than the Ga atoms. Successful doping of BaGa2Sb2 with Na or K was confirmed with combined microprobe and X-ray diffraction analysis. Alkali metal doping of BaGa2Sb2 increased the p-type charge carrier concentration to almost the predicted optimum values (similar to 10(20) h(+) cm(-3)) needed to achieve high thermoelectric performance. With increasing alkali metal concentration, electronic transport was shifted from non-degenerate semiconducting behaviour observed for BaGa2Sb2 to degenerate one for Na- or K-doped compounds. Overall, the thermoelectric figure of merit, zT, values reached up to similar to 0.65 at 750 K, considerably higher than the undoped sample (zT similar to 0.1 at 600 K), and a slight improvement relative to previously reported Zn-doped samples (similar to 0.6 at 800 K).
C1 [Aydemir, Umut; Snyder, G. Jeffrey] CALTECH, Dept Appl Phys & Mat Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Aydemir, Umut; Snyder, G. Jeffrey] Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
[Zevalkink, Alex; Bux, Sabah] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zevalkink, Alex; Ormeci, Alim] Max Planck Inst Chem Phys Solids, Nothnitzer Str 40, D-01187 Dresden, Germany.
RP Aydemir, U (reprint author), CALTECH, Dept Appl Phys & Mat Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.; Aydemir, U (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
EM umut.aydemir@northwestern.edu
RI Snyder, G. Jeffrey/E-4453-2011; Ormeci, Alim/F-1082-2012
OI Snyder, G. Jeffrey/0000-0003-1414-8682; Ormeci, Alim/0000-0001-5468-3378
FU Scientific and Technological Research Council of Turkey; NASA Science
Missions Directorate's Radioisotope Power Systems Technology Advancement
Program
FX U. A. acknowledges the financial assistance of The Scientific and
Technological Research Council of Turkey. This research was carried out
in part at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration and was supported by the NASA Science Missions
Directorate's Radioisotope Power Systems Technology Advancement Program.
We would like to acknowledge the Molecular Materials Research Center
(MMRC) at Caltech for allowing use of their instruments for the optical
measurements obtained in this work. A. O. thanks Ulrike Nitzsche from
IFW Dresden, Germany for technical help in computational work.
NR 56
TC 5
Z9 5
U1 11
U2 33
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2050-7488
EI 2050-7496
J9 J MATER CHEM A
JI J. Mater. Chem. A
PY 2016
VL 4
IS 5
BP 1867
EP 1875
DI 10.1039/c5ta07612a
PG 9
WC Chemistry, Physical; Energy & Fuels; Materials Science,
Multidisciplinary
SC Chemistry; Energy & Fuels; Materials Science
GA DB9MC
UT WOS:000368839200038
ER
PT J
AU Anderson, DC
Nicely, JM
Salawitch, RJ
Canty, TP
Dickerson, RR
Hanisco, TF
Wolfe, GM
Apel, EC
Atlas, E
Bannan, T
Bauguitte, S
Blake, NJ
Bresch, JF
Campos, TL
Carpenter, LJ
Cohen, MD
Evans, M
Fernandez, RP
Kahn, BH
Kinnison, DE
Hall, SR
Harris, NRP
Hornbrook, RS
Lamarque, JF
Le Breton, M
Lee, JD
Percival, C
Pfister, L
Pierce, RB
Riemer, DD
Saiz-Lopez, A
Stunder, BJB
Thompson, AM
Ullmann, K
Vaughan, A
Weinheimer, AJ
AF Anderson, Daniel C.
Nicely, Julie M.
Salawitch, Ross J.
Canty, Timothy P.
Dickerson, Russell R.
Hanisco, Thomas F.
Wolfe, Glenn M.
Apel, Eric C.
Atlas, Elliot
Bannan, Thomas
Bauguitte, Stephane
Blake, Nicola J.
Bresch, James F.
Campos, Teresa L.
Carpenter, Lucy J.
Cohen, Mark D.
Evans, Mathew
Fernandez, Rafael P.
Kahn, Brian H.
Kinnison, Douglas E.
Hall, Samuel R.
Harris, Neil R. P.
Hornbrook, Rebecca S.
Lamarque, Jean-Francois
Le Breton, Michael
Lee, James D.
Percival, Carl
Pfister, Leonhard
Pierce, R. Bradley
Riemer, Daniel D.
Saiz-Lopez, Alfonso
Stunder, Barbara J. B.
Thompson, Anne M.
Ullmann, Kirk
Vaughan, Adam
Weinheimer, Andrew J.
TI A pervasive role for biomass burning in tropical high ozone/low water
structures
SO NATURE COMMUNICATIONS
LA English
DT Article
ID EQUATORIAL PACIFIC-OCEAN; REMOTE SOUTH-PACIFIC; TROPOSPHERIC OZONE;
WESTERN PACIFIC; ATMOSPHERIC CHEMISTRY; PEM-TROPICS; LOWER STRATOSPHERE;
HYDROGEN-CYANIDE; DRY AIR; MODEL
AB Air parcels with mixing ratios of high O-3 and low H2O (HOLW) are common features in the tropical western Pacific (TWP) mid-troposphere (300-700 hPa). Here, using data collected during aircraft sampling of the TWP in winter 2014, we find strong, positive correlations of O-3 with multiple biomass burning tracers in these HOLW structures. Ozone levels in these structures are about a factor of three larger than background. Models, satellite data and aircraft observations are used to show fires in tropical Africa and Southeast Asia are the dominant source of high O-3 and that low H2O results from large-scale descent within the tropical troposphere. Previous explanations that attribute HOLW structures to transport from the stratosphere or mid-latitude troposphere are inconsistent with our observations. This study suggest a larger role for biomass burning in the radiative forcing of climate in the remote TWP than is commonly appreciated.
C1 [Anderson, Daniel C.; Salawitch, Ross J.; Canty, Timothy P.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Nicely, Julie M.; Salawitch, Ross J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
[Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Hanisco, Thomas F.; Wolfe, Glenn M.; Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Apel, Eric C.; Campos, Teresa L.; Kinnison, Douglas E.; Hall, Samuel R.; Hornbrook, Rebecca S.; Lamarque, Jean-Francois; Ullmann, Kirk; Weinheimer, Andrew J.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, Boulder, CO 80305 USA.
[Atlas, Elliot; Riemer, Daniel D.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
[Bannan, Thomas; Le Breton, Michael; Percival, Carl] Univ Manchester, Ctr Atmospher Sci, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England.
[Bauguitte, Stephane] Facil Airborne Atmospher Measurements, Cranfield MK43 0JR, Beds, England.
[Blake, Nicola J.] Univ Calif Irvine, Deparment Chem, Irvine, CA 92697 USA.
[Bresch, James F.] Natl Ctr Atmospher Res, Mesoscale & Microscale Meteorol Lab, Boulder, CO 80305 USA.
[Carpenter, Lucy J.; Evans, Mathew] Univ York, Dept Chem, Wolfson Atmospher Chem Labs, York YO10 5DD, N Yorkshire, England.
[Cohen, Mark D.; Stunder, Barbara J. B.] NOAA, Air Resources Lab, College Pk, MD 20740 USA.
[Evans, Mathew; Lee, James D.; Vaughan, Adam] Univ York, Dept Chem, Natl Ctr Atmospher Sci, York YO10 5DD, N Yorkshire, England.
[Fernandez, Rafael P.; Saiz-Lopez, Alfonso] CSIC, Inst Phys Chem Rocasolano, Dept Atmospher Chem & Climate, Plaza Murillo 2, E-28006 Madrid, Spain.
[Fernandez, Rafael P.] FCEN UNCuyo, Natl Res Council CONICET, Dept Nat Sci, RA-5501 Mendoza, Argentina.
[Kahn, Brian H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Harris, Neil R. P.] Univ Cambridge, Dept Chem, Lensfield Rd, Cambridge CB2 1EW, England.
[Lamarque, Jean-Francois] Natl Ctr Atmospher Res, Climate & Global Dynam Lab, Boulder, CO 80305 USA.
[Pfister, Leonhard] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Pierce, R. Bradley] NOAA NESDIS Ctr Satellite Applicat & Res, Madison, WI 53706 USA.
RP Anderson, DC (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM danderson@atmos.umd.edu
RI Nicely, Julie/E-3668-2016; Pierce, Robert Bradley/F-5609-2010; Wolfe,
Glenn/D-5289-2011; Saiz-Lopez, Alfonso/B-3759-2015; Lamarque,
Jean-Francois/L-2313-2014; Anderson, Daniel/I-4398-2014; Dickerson,
Russell/F-2857-2010; Salawitch, Ross/B-4605-2009; Evans,
Mathew/A-3886-2012; Vaughan, Adam/O-2912-2015; Canty,
Timothy/F-2631-2010;
OI Harris, Neil/0000-0003-1256-3006; Nicely, Julie/0000-0003-4828-0032;
Pierce, Robert Bradley/0000-0002-2767-1643; Saiz-Lopez,
Alfonso/0000-0002-0060-1581; Lamarque,
Jean-Francois/0000-0002-4225-5074; Anderson, Daniel/0000-0002-9826-9811;
Dickerson, Russell/0000-0003-0206-3083; Salawitch,
Ross/0000-0001-8597-5832; Evans, Mathew/0000-0003-4775-032X; Vaughan,
Adam/0000-0002-7878-0719; Canty, Timothy/0000-0003-0618-056X; Cohen,
Mark/0000-0003-3183-2558
FU Natural Environment Research Council; National Science Foundation;
National Aeronautics and Space Administration (NASA); National Oceanic
and Atmospheric Administration
FX We thank L. Pan for coordinating the CONTRAST flights and her
constructive criticism of an early version of the manuscript; S.
Schauffler, V. Donets and R. Lueb for collecting and analysing AWAS
samples; T. Robinson and O. Shieh for providing meteorology forecasts in
the field; and the pilots and crews of the CAST BAe-146 and CONTRAST
Gulfstream V aircrafts for their dedication and professionalism. CAST
was funded by the Natural Environment Research Council; CONTRAST was
funded by the National Science Foundation. Research at the Jet
Propulsion Laboratory, California Institute of Technology, is performed
under contract with the National Aeronautics and Space Administration
(NASA). A number of the US-based investigators also benefitted from the
support of NASA as well as the National Oceanic and Atmospheric
Administration. The views, opinions, and findings contained in this
report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or US
Government position, policy or decision. We would like to acknowledge
high-performance computing support from Yellowstone
(ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information
Systems Laboratory. NCAR is sponsored by the National Science
Foundation.
NR 70
TC 6
Z9 6
U1 6
U2 21
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 JAN
PY 2016
VL 7
AR 10267
DI 10.1038/ncomms10267
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC2AX
UT WOS:000369020700002
PM 26758808
ER
PT J
AU Boixo, S
Smelyanskiy, VN
Shabani, A
Isakov, SV
Dykman, M
Denchev, VS
Amin, MH
Smirnov, AY
Mohseni, M
Neven, H
AF Boixo, Sergio
Smelyanskiy, Vadim N.
Shabani, Alireza
Isakov, Sergei V.
Dykman, Mark
Denchev, Vasil S.
Amin, Mohammad H.
Smirnov, Anatoly Yu.
Mohseni, Masoud
Neven, Hartmut
TI Computational multiqubit tunnelling in programmable quantum annealers
SO NATURE COMMUNICATIONS
LA English
DT Article
ID ISING-MODEL
AB Quantum tunnelling is a phenomenon in which a quantum state traverses energy barriers higher than the energy of the state itself. Quantum tunnelling has been hypothesized as an advantageous physical resource for optimization in quantum annealing. However, computational multiqubit tunnelling has not yet been observed, and a theory of co-tunnelling under high-and low-frequency noises is lacking. Here we show that 8-qubit tunnelling plays a computational role in a currently available programmable quantum annealer. We devise a probe for tunnelling, a computational primitive where classical paths are trapped in a false minimum. In support of the design of quantum annealers we develop a nonperturbative theory of open quantum dynamics under realistic noise characteristics. This theory accurately predicts the rate of many-body dissipative quantum tunnelling subject to the polaron effect. Furthermore, we experimentally demonstrate that quantum tunnelling outperforms thermal hopping along classical paths for problems with up to 200 qubits containing the computational primitive.
C1 [Boixo, Sergio; Smelyanskiy, Vadim N.; Shabani, Alireza; Isakov, Sergei V.; Denchev, Vasil S.; Mohseni, Masoud; Neven, Hartmut] Google, Venice, CA 90291 USA.
[Smelyanskiy, Vadim N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dykman, Mark] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Amin, Mohammad H.; Smirnov, Anatoly Yu.] D Wave Syst Inc, Burnaby, BC V5C 6G9, Canada.
[Amin, Mohammad H.] Simon Fraser Univ, Dept Phys, Burnaby, BC V5A 1S6, Canada.
RP Boixo, S; Smelyanskiy, VN (reprint author), Google, Venice, CA 90291 USA.; Smelyanskiy, VN (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM boixo@google.com; smelyan@google.com
FU Office of the Director of National Intelligence (ODNI), Intelligence
Advanced Research Projects Activity (IARPA) [IAA 145483]; AFRL
Information Directorate [F4HBKC4162G001]
FX We thank John Martinis, Edward Farhi and Anthony Leggett for useful
discussions and reviewing the manuscript. We also thank Ryan Babbush and
Bryan O'Gorman for reviewing the manuscript, and Damian Steiger, Daniel
Lidar and Tameem Albash for comments about the temperature experiment.
The work of V. N. S. was supported in part by the Office of the Director
of National Intelligence (ODNI), Intelligence Advanced Research Projects
Activity (IARPA) via IAA 145483 and by the AFRL Information Directorate
under grant F4HBKC4162G001.
NR 37
TC 19
Z9 19
U1 2
U2 13
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 JAN
PY 2016
VL 7
AR 10327
DI 10.1038/ncomms10327
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC2BG
UT WOS:000369021600002
PM 26739797
ER
PT J
AU Yi, X
Vahala, K
Li, J
Diddams, S
Ycas, G
Plavchan, P
Leifer, S
Sandhu, J
Vasisht, G
Chen, P
Gao, P
Gagne, J
Furlan, E
Bottom, M
Martin, EC
Fitzgerald, MP
Doppmann, G
Beichman, C
AF Yi, X.
Vahala, K.
Li, J.
Diddams, S.
Ycas, G.
Plavchan, P.
Leifer, S.
Sandhu, J.
Vasisht, G.
Chen, P.
Gao, P.
Gagne, J.
Furlan, E.
Bottom, M.
Martin, E. C.
Fitzgerald, M. P.
Doppmann, G.
Beichman, C.
TI Demonstration of a near-IR line-referenced electro-optical laser
frequency comb for precision radial velocity measurements in astronomy
SO NATURE COMMUNICATIONS
LA English
DT Article
ID PHASE; FIBER; GENERATION; SPECTROGRAPHS; CALIBRATION; MODULATION;
EXOPLANETS
AB An important technique for discovering and characterizing planets beyond our solar system relies upon measurement of weak Doppler shifts in the spectra of host stars induced by the influence of orbiting planets. A recent advance has been the introduction of optical frequency combs as frequency references. Frequency combs produce a series of equally spaced reference frequencies and they offer extreme accuracy and spectral grasp that can potentially revolutionize exoplanet detection. Here we demonstrate a laser frequency comb using an alternate comb generation method based on electro-optical modulation, with the comb centre wavelength stabilized to a molecular or atomic reference. In contrast to mode-locked combs, the line spacing is readily resolvable using typical astronomical grating spectrographs. Built using commercial off-the-shelf components, the instrument is relatively simple and reliable. Proof of concept experiments operated at near-infrared wavelengths were carried out at the NASA Infrared Telescope Facility and the Keck-II telescope.
C1 [Yi, X.; Vahala, K.; Li, J.] Dept Appl Phys & Mat Sci, Pasadena, CA 91125 USA.
[Diddams, S.; Ycas, G.] NIST, 325 Broadway, Boulder, CO 80305 USA.
[Diddams, S.; Ycas, G.] Univ Colorado, Dept Phys, 2000 Colorado Ave, Boulder, CO 80309 USA.
[Plavchan, P.] Missouri State Univ, Dept Phys, 901 S Natl Ave, Springfield, MO 65897 USA.
[Leifer, S.; Sandhu, J.; Vasisht, G.; Chen, P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gao, P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Gagne, J.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd, Washington, DC 20015 USA.
[Furlan, E.; Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bottom, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Martin, E. C.; Fitzgerald, M. P.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Doppmann, G.] WM Keck Observ, Kamuela, HI 96743 USA.
RP Vahala, K (reprint author), Dept Appl Phys & Mat Sci, Pasadena, CA 91125 USA.; Beichman, C (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
EM vahala@caltech.edu; chas@ipac.caltech.edu
RI Chen, Pin/B-1112-2008;
OI Chen, Pin/0000-0003-1195-9666; Fitzgerald, Michael/0000-0002-0176-8973
FU W.M. Keck Foundation; NIST; NSF [AST-1310875]; President's and
Director's Fund Program
FX Three IRTF nights were donated in September 2014 to integrate and test
the laser comb with CSHELL. One of these nights came from IRTF
engineering time and the other two came from Peter Plavchan's CSHELL
program to observe nearby M dwarfs with the absorption gas cell to
obtain precise radial velocities. We are grateful to the leadership of
the IRTF, Director Alan Tokunaga and Deputy Director John Rayner, as
well as to the daytime and night time staff at the summit for their
support. We further thank Jeremy Colson at Wavelength References for his
assistance with the molecular-stabilized lasers. On-sky observations
were obtained at the Infrared Telescope Facility, which is operated by
the University of Hawaii under Cooperative Agreement no. NNX-08AE38A
with the National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program. Daytime operations at the
Keck-II telescope were carried out with the assistance of Sean Adkins
and Steve Milner. We greatfully acknowledge the support of the entire
Keck summit team in making these tests possible. We recognize and
acknowledge the very significant cultural role and reverence 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. 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
Observatory was made possible by the generous financial support of the
W.M. Keck Foundation. We also acknowledge support from NIST and the NSF
grant AST-1310875. This research was carried out at the Jet Propulsion
Laboratory and the California Institute of Technology under a contract
with the National Aeronautics and Space Administration and funded
through the President's and Director's Fund Program. Copyright 2014
California Institute of Technology. All rights reserved.
NR 39
TC 5
Z9 5
U1 10
U2 30
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 JAN
PY 2016
VL 7
AR 10436
DI 10.1038/ncomms10436
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DC2BQ
UT WOS:000369022600019
PM 26813804
ER
PT S
AU Paoli, R
Shariff, K
AF Paoli, Roberto
Shariff, Karim
BE Davis, SH
Moin, P
TI Contrail Modeling and Simulation
SO ANNUAL REVIEW OF FLUID MECHANICS, VOL 48
SE Annual Review of Fluid Mechanics
LA English
DT Review; Book Chapter
DE two-phase flow; particulate flows; vortex dynamics; stratified flow;
cloud formation and dynamics; large-eddy simulation; radiative
hydrodynamics
ID LARGE-EDDY SIMULATION; TO-CIRRUS TRANSITION; IN-SITU OBSERVATIONS;
RADIATIVE PROPERTIES; VORTEX PHASE; NUMERICAL SIMULATIONS; AIRCRAFT
WAKES; CLIMATE MODELS; ICE PARTICLES; AERODYNAMIC CONTRAILS
AB There is large uncertainty in the radiative forcing induced by aircraft contrails, particularly after they transform to cirrus. It has recently become possible to simulate contrail evolution for long periods after their formation. We review the main physical processes and simulation efforts in the four phases of contrail evolution, namely the jet, vortex, vortex dissipation, and diffusion phases. Recommendations for further work are given.
C1 [Paoli, Roberto] CERFACS, F-31057 Toulouse 01, France.
[Shariff, Karim] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Paoli, Roberto] Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA.
[Paoli, Roberto] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
RP Paoli, R (reprint author), CERFACS, F-31057 Toulouse 01, France.; Shariff, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Paoli, R (reprint author), Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA.; Paoli, R (reprint author), Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
EM paoli@cerfacs.fr; karim.shariff@nasa.gov
OI Shariff, Karim/0000-0002-7256-2497
NR 163
TC 4
Z9 4
U1 2
U2 14
PU ANNUAL REVIEWS
PI PALO ALTO
PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA
SN 0066-4189
BN 978-0-8243-0748-6
J9 ANNU REV FLUID MECH
JI Annu. Rev. Fluid Mech.
PY 2016
VL 48
BP 393
EP 427
DI 10.1146/annurev-fluid-010814-013619
PG 35
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA BE1QA
UT WOS:000368367800016
ER
PT J
AU Grazier, KR
AF Grazier, Kevin R.
TI Jupiter: Cosmic Jekyll and Hyde
SO ASTROBIOLOGY
LA English
DT Article
ID OUTER SOLAR-SYSTEM; PERMIAN MASS EXTINCTION; OORT CLOUD; DYNAMICAL
EVOLUTION; GIANT IMPACT; COMETS; FRIEND; FOE; ORIGIN; BODIES
AB It has been widely reported that Jupiter has a profound role in shielding the terrestrial planets from comet impacts in the Solar System, and that a jovian planet is a requirement for the evolution of life on Earth. To evaluate whether jovians, in fact, shield habitable planets from impacts (a phenomenon often referred to as the Jupiter as shield concept), this study simulated the evolution of 10,000 particles in each of the jovian inter-planet gaps for the cases of full-mass and embryo planets for up to 100 My. The results of these simulations predict a number of phenomena that not only discount the Jupiter as shield concept, they also predict that in a Solar System like ours, large gas giants like Saturn and Jupiter had a different, and potentially even more important, role in the evolution of life on our planet by delivering the volatile-laden material required for the formation of life. The simulations illustrate that, although all particles occupied non-life threatening orbits at their onset of the simulations, a significant fraction of the 30,000 particles evolved into Earth-crossing orbits. A comparison of multiple runs with different planetary configurations revealed that Jupiter was responsible for the vast majority of the encounters that kicked outer planet material into the terrestrial planet region, and that Saturn assisted in the process far more than has previously been acknowledged. Jupiter also tends to fix the aphelion of planetesimals at its orbit irrespective of their initial starting zones, which has the effect of slowing their passages through the inner Solar System, and thus potentially improving the odds of accretion of cometary material by terrestrial planets. As expected, the simulations indicate that the full-mass planets perturb many objects into the deep outer Solar System, or eject them entirely; however, planetary embryos also did this with surprising efficiency. Finally, the simulations predict that Jupiter's capacity to shield or intercept Earth-bound comets originating in the outer Solar System is poor, and that the importance of jovian planets on the formation of life is not that they act as shields, but rather that they deliver life-enabling volatiles to the terrestrial planets. Key Words: AsteroidCometsInterstellar meteoritesExtrasolar terrestrial planetsSimulation. Astrobiology 16, 23-38.
C1 [Grazier, Kevin R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Grazier, KR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM kevin_grazier@yahoo.com
NR 67
TC 1
Z9 1
U1 4
U2 6
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 JAN 1
PY 2016
VL 16
IS 1
BP 23
EP 38
DI 10.1089/ast.2015.1321
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DB7QB
UT WOS:000368709500003
PM 26701303
ER
PT J
AU Belavy, DL
Adams, M
Brisby, H
Cagnie, B
Danneels, L
Fairbank, J
Hargens, AR
Judex, S
Scheuring, RA
Sovelius, R
Urban, J
van Dieen, JH
Wilke, HJ
AF Belavy, Daniel L.
Adams, Michael
Brisby, Helena
Cagnie, Barbara
Danneels, Lieven
Fairbank, Jeremy
Hargens, Alan R.
Judex, Stefan
Scheuring, Richard A.
Sovelius, Roope
Urban, Jill
van Dieen, Jaap H.
Wilke, Hans-Joachim
TI Disc herniations in astronauts: What causes them, and what does it tell
us about herniation on earth?
SO EUROPEAN SPINE JOURNAL
LA English
DT Review
DE Prolapse; Atrophy; Back pain; Muscle; Inactivity; Bed rest
ID HUMAN INTERVERTEBRAL DISC; PROLONGED BED REST; WHOLE-BODY VIBRATION;
LUMBAR SPINE; IN-VIVO; NUCLEUS PULPOSUS; SIMULATED MICROGRAVITY;
VERTEBRAL BODIES; ANULUS FIBROSUS; SYNTHESIS RATES
AB Recent work showed an increased risk of cervical and lumbar intervertebral disc (IVD) herniations in astronauts. The European Space Agency asked the authors to advise on the underlying pathophysiology of this increased risk, to identify predisposing factors and possible interventions and to suggest research priorities.
The authors performed a narrative literature review of the possible mechanisms, and conducted a survey within the team to prioritize research and prevention approaches.
Based on literature review the most likely cause for lumbar IVD herniations was concluded to be swelling of the IVD in the unloaded condition during spaceflight. For the cervical IVDs, the knowledge base is too limited to postulate a likely mechanism or recommend approaches for prevention. Basic research on the impact of (un)loading on the cervical IVD and translational research is needed. The highest priority prevention approach for the lumbar spine was post-flight care avoiding activities involving spinal flexion, followed by passive spinal loading in spaceflight and exercises to reduce IVD hyper-hydration post-flight.
C1 [Belavy, Daniel L.] Charite, Ctr Muscle & Bone Res, Hindenburgdamm 30, D-12203 Berlin, Germany.
[Belavy, Daniel L.] Deakin Univ, Sch Exercise & Nutr Sci, Ctr Phys Activ & Nutr Res, 221 Burwood Highway, Burwood, Vic 3125, Australia.
[Adams, Michael] Univ Bristol, Ctr Comparat & Clin Anat, Southwell St, Bristol BS2 8EJ, Avon, England.
[Brisby, Helena] Gothenburg Univ, Sahlgrenska Acad, Inst Clin Sci, Dept Orthoped, Gothenburg, Sweden.
[Brisby, Helena] Sahlgrens Univ Hosp, Dept Orthoped, Gothenburg, Sweden.
[Cagnie, Barbara; Danneels, Lieven] Univ Ghent, Dept Rehabil Sci & Physiotherapy, De Pintelaan 185 3B3, B-9000 Ghent, Belgium.
[Fairbank, Jeremy] Oxford Univ Hosp NHS Trust, Headington, Nuffield Orthopaed Ctr, Oxford OX3 7HE, England.
[Hargens, Alan R.] Univ Calif San Diego, Dept Orthopaed Surg, San Diego, CA 92103 USA.
[Judex, Stefan] SUNY Stony Brook, Bioengn Bldg, Stony Brook, NY 11794 USA.
[Scheuring, Richard A.] Lyndon B Johnson Space Ctr, 2101 NASA Pkwy SD4, Houston, TX 77058 USA.
[Sovelius, Roope] Satakunta Air Command, Ctr Mil Med, POB 1000, Pirkkala 33961, Finland.
[Urban, Jill] Univ Oxford, Dept Physiol Anat & Genet, Le Gros Clark Bldg,South Pk Rd, Oxford OX1 3QX, England.
[van Dieen, Jaap H.] Vrije Univ Amsterdam, MOVE Res Inst Amsterdam, Fac Human Movement Sci, Boechorststr 9, NL-1081 BT Amsterdam, Netherlands.
[Wilke, Hans-Joachim] Univ Ulm, Inst Orthopaed Res & Biomech, Helmholtzstr 14, D-89081 Ulm, Germany.
RP Belavy, DL (reprint author), Charite, Ctr Muscle & Bone Res, Hindenburgdamm 30, D-12203 Berlin, Germany.; Belavy, DL (reprint author), Deakin Univ, Sch Exercise & Nutr Sci, Ctr Phys Activ & Nutr Res, 221 Burwood Highway, Burwood, Vic 3125, Australia.
EM belavy@gmail.com; M.A.Adams@bristol.ac.uk; helena.brisby@vgregion.se;
barbara.cagnie@ugent.be; Lieven.Danneels@ugent.be;
jeremy.fairbank@ndorms.ox.ac.uk; ahargens@ucsd.edu;
stefan.judex@stonybrook.edu; richard.a.scheuring@nasa.gov;
roope.sovelius@mil.fi; jill.urban@dpag.ox.ac.uk; j.van.dieen@vu.nl;
hans-joachim.wilke@uni-ulm.de
RI Belavy, Daniel/P-4947-2016; Wilke, Hans-Joachim/M-6440-2014; cagnie,
barbara/D-9830-2017;
OI Belavy, Daniel/0000-0002-9307-832X; cagnie, barbara/0000-0003-4342-4519;
Hargens, Alan/0000-0002-4722-1375
FU European Space Agency [4000110441/14/NL/PG]; NASA [NNX13AM89G]
FX We thank our colleagues at the European Space Agency, Dr. Oliver Angerer
and Dr. Jennifer Ngo-An, for facilitating our discussions. DLB thanks
Dr. Zully Ritter for assistance in generating Fig. 2. We acknowledge the
assistance of our colleagues at the European Astronaut Centre for
clarifying our questions regarding astronaut training and care. The
"European Space Agency Topical Team: Intervertebral Disc Herniations in
Astronauts" was supported by contract number 4000110441/14/NL/PG from
the European Space Agency. ARH was supported by NASA grant NNX13AM89G.
NR 75
TC 7
Z9 7
U1 4
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0940-6719
EI 1432-0932
J9 EUR SPINE J
JI Eur. Spine J.
PD JAN
PY 2016
VL 25
IS 1
BP 144
EP 154
DI 10.1007/s00586-015-3917-y
PG 11
WC Clinical Neurology; Orthopedics
SC Neurosciences & Neurology; Orthopedics
GA DB6FI
UT WOS:000368608900016
PM 25893331
ER
PT S
AU Rouse, M
Jegley, D
AF Rouse, Marshall
Jegley, Dawn
BE Sciammarella, C
Considine, J
Gloeckner, P
TI Testing a Multi-bay Box Subjected to Combined Loads
SO EXPERIMENTAL AND APPLIED MECHANICS, VOL 4
SE Conference Proceedings of the Society for Experimental Mechanics Series
LA English
DT Proceedings Paper
CT Annual Conference and Exposition of Society-for-Experimental-Mechanics
on Experimental and Applied Mechanics
CY JUN 08-11, 2015
CL Costa Mesa, CA
SP Soc Experimental Mech
DE Composite; Combined loading; Hybrid wing body; PRSEUS; Rod-stiffened
AB The COmbined Loads Test System (COLTS) facility at NASA Langley Research Center provides a test capability to help develop validated structures technologies. The test machine was design to accommodate a range of fuselage structures and wing sections and subject them to both quasistatic and cyclic loading conditions. The COLTS facility is capable of testing fuselage barrels up to 4.6 m in diameter and 13.7 m long with combined mechanical, internal pressure, and thermal loads. The COLTS facility is currently being prepared to conduct a combined mechanical and pressure loading for a multi-bay pressure box to experimentally verify the structural performance of a composite structure which is 9.1 m long and representative of a section of a hybrid wing body fuselage section in support of the Environmentally Responsible Aviation Project at NASA. This paper describes development of the multi-bay pressure box test using the COLTS facility. The multi-bay test article will be subjected to mechanical loads and internal pressure loads up to design ultimate load. Mechanical and pressure loads will be applied independently in some tests and simultaneously in others.
C1 [Rouse, Marshall; Jegley, Dawn] NASA, Langley Res Ctr, Mail Stop 190, Hampton, VA 23681 USA.
RP Rouse, M (reprint author), NASA, Langley Res Ctr, Mail Stop 190, Hampton, VA 23681 USA.
EM marshal.rouse@nasa.gov; dawn.c.jegley@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 2191-5644
BN 978-3-319-22449-7; 978-3-319-22448-0
J9 C PROC SOC EXP MECH
PY 2016
BP 173
EP 182
DI 10.1007/978-3-319-22449-7_21
PG 10
WC Mechanics
SC Mechanics
GA BE1UI
UT WOS:000368587400021
ER
PT J
AU Caldwell, PM
Zelinka, MD
Taylor, KE
Marvel, K
AF Caldwell, Peter M.
Zelinka, Mark D.
Taylor, Karl E.
Marvel, Kate
TI Quantifying the Sources of Intermodel Spread in Equilibrium Climate
Sensitivity
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Physical Meteorology and Climatology; Climate sensitivity; Feedback;
Forcing; Mathematical and statistical techniques; Statistics; Models and
modeling; Climate models
ID RADIATIVE KERNEL TECHNIQUE; OCEAN-ATMOSPHERE MODELS; FEEDBACK;
DEPENDENCE; CLOUDS; ECMWF; CO2
AB This study clarifies the causes of intermodel differences in the global-average temperature response to doubled CO2, commonly known as equilibrium climate sensitivity (ECS). The authors begin by noting several issues with the standard approach for decomposing ECS into a sum of forcing and feedback terms. This leads to a derivation of an alternative method based on linearizing the effect of the net feedback. Consistent with previous studies, the new method identifies shortwave cloud feedback as the dominant source of intermodel spread in ECS. This new approach also reveals that covariances between cloud feedback and forcing, between lapse rate and longwave cloud feedbacks, and between albedo and shortwave cloud feedbacks play an important and previously underappreciated role in determining model differences in ECS. Defining feedbacks based on fixed relative rather than specific humidity (as suggested by Held and Shell) reduces the covariances between processes and leads to more straightforward interpretations of results.
C1 [Caldwell, Peter M.; Zelinka, Mark D.; Taylor, Karl E.; Marvel, Kate] Lawrence Livermore Natl Lab, L-103,POB 808, Livermore, CA 94566 USA.
[Marvel, Kate] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Caldwell, PM (reprint author), Lawrence Livermore Natl Lab, L-103,POB 808, Livermore, CA 94566 USA.
EM caldwell19@llnl.gov
RI Taylor, Karl/F-7290-2011; Zelinka, Mark/C-4627-2011
OI Taylor, Karl/0000-0002-6491-2135; Zelinka, Mark/0000-0002-6570-5445
FU Office of Science (BER) at Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; BER's Regional and Global Climate Modeling (RGCM)
Program
FX We would like to acknowledge the modeling groups [the Program for
Climate Model Diagnosis and Intercomparison (PCMDI) and the World
Climate Research Programme's Working Group on Coupled Modelling] for
their roles in making available the CMIP5 multimodel dataset. Thanks
also go to Thomas Reichler for making his WMO tropopause code publicly
available. Support for these datasets is provided by the U.S. Department
of Energy (DOE) Office of Science. This work was supported by the Office
of Science (BER) at Lawrence Livermore National Laboratory under
Contract DE-AC52-07NA27344. All authors were supported by BER's Regional
and Global Climate Modeling (RGCM) Program.
NR 38
TC 2
Z9 2
U1 3
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD JAN
PY 2016
VL 29
IS 2
BP 513
EP 524
DI 10.1175/JCLI-D-15-0352.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB6OH
UT WOS:000368633800001
ER
PT J
AU Ye, HC
Fetzer, EJ
Behrangi, A
Wong, S
Lambrigtsen, BH
Wang, CY
Cohen, J
Gamelin, BL
AF Ye, Hengchun
Fetzer, Eric J.
Behrangi, Ali
Wong, Sun
Lambrigtsen, Bjorn H.
Wang, Crysti Y.
Cohen, Judah
Gamelin, Brandi L.
TI Increasing Daily Precipitation Intensity Associated with Warmer Air
Temperatures over Northern Eurasia
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Geographic location; entity; Arctic; Physical Meteorology and
Climatology; Climate change; Mixed precipitation; Variability; Arctic
Oscillation; Climate variability; Interdecadal variability
ID ATMOSPHERIC CIRCULATION; ARCTIC OSCILLATION; CLIMATE-CHANGE; STORM
TRACKS; FREQUENCY; EXTREMES; TRENDS; MODEL; SIMULATIONS; PROJECTIONS
AB This study uses 45 years of observational records from 517 historical surface weather stations over northern Eurasia to examine changing precipitation characteristics associated with increasing air temperatures. Results suggest that warming air temperatures over northern Eurasia have been accompanied by higher precipitation intensity but lower frequency and little change in annual precipitation total. An increase in daily precipitation intensity of around 1%-3% per each degree of air temperature increase is found for all seasons as long as a station's seasonal mean air temperature is below about 15 degrees-16 degrees C. This threshold temperature may be location dependent. At temperatures above this threshold, precipitation intensity switches to decreasing with increasing air temperature, possibly related to decreasing water vapor associated with extreme high temperatures. Furthermore, the major atmospheric circulation of the Arctic Oscillation, Scandinavian pattern, east Atlantic-western Eurasian pattern, and polar-Eurasian pattern also have significant influences on precipitation intensity in winter, spring, and summer over certain areas of northern Eurasia.
C1 [Ye, Hengchun] Calif State Univ Los Angeles, Dept Geosci & Environm, 5151 State Univ Dr, Los Angeles, CA 90032 USA.
[Fetzer, Eric J.; Behrangi, Ali; Wong, Sun; Lambrigtsen, Bjorn H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wang, Crysti Y.] Wellesley Coll, Wellesley, MA 02181 USA.
[Cohen, Judah] Atmospher & Environm Res Inc, Lexington, MA USA.
[Gamelin, Brandi L.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
RP Ye, HC (reprint author), Calif State Univ Los Angeles, Dept Geosci & Environm, 5151 State Univ Dr, Los Angeles, CA 90032 USA.
EM hye2@calstatela.edu
FU NSF [BCS-1060788, BCS-106033]; NASA [NNX15AQ06A]; NASA JPL AIRS project;
NASA MeaSUREs project; NASA Earth System Data Record Uncertainty
Analysis project
FX The first author is supported by NSF Grant BCS-1060788, and the seventh
author is supported by NSF Grant BCS-106033. Some 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. The first author and
the JPL authors are supported by NASA Grant NNX15AQ06A, the NASA JPL
AIRS project, the NASA MeaSUREs project, and the NASA Earth System Data
Record Uncertainty Analysis project.
NR 48
TC 3
Z9 3
U1 3
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD JAN
PY 2016
VL 29
IS 2
BP 623
EP 636
DI 10.1175/JCLI-D-14-00771.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB6PD
UT WOS:000368636100004
ER
PT J
AU Ray, RD
Zaron, ED
AF Ray, R. D.
Zaron, E. D.
TI M-2 Internal Tides and Their Observed Wavenumber Spectra from Satellite
Altimetry
SO JOURNAL OF PHYSICAL OCEANOGRAPHY
LA English
DT Article
DE Atm; Ocean Structure; Phenomena; Tides; Observational techniques and
algorithms; Satellite observations
ID NORTH PACIFIC; OCEAN; TOPEX/POSEIDON; RIDGE; CIRCULATION; TOPOGRAPHY;
MISSION; HAWAII; MODEL
AB A near-global chart of surface elevations associated with the stationary M-2 internal tide is empirically constructed from multimission satellite altimeter data. An advantage of a strictly empirical mapping approach is that results are independent of assumptions about ocean wave dynamics and, in fact, can be used to test such assumptions. A disadvantage is that present-day altimeter coverage is only marginally adequate to support mapping such short-wavelength features. Moreover, predominantly north-south ground-track orientations and contamination from nontidal oceanographic variability can lead to deficiencies in mapped tides. Independent data from Cryosphere Satellite-2 (CryoSat-2) and other altimeters are used to test the solutions and show positive reduction in variance except in regions of large mesoscale variability. The tidal fields are subjected to two-dimensional wavenumber spectral analysis, which allows for the construction of an empirical map of modal wavelengths. Mode-1 wavelengths show good agreement with theoretical wavelengths calculated from the ocean's mean stratification, with a few localized exceptions (e.g., Tasman Sea). Mode-2 waves are detectable in much of the ocean, with wavelengths in reasonable agreement with theoretical expectations, but their spectral signatures grow too weak to map in some regions.
C1 [Ray, R. D.] NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
[Zaron, E. D.] Portland State Univ, Dept Civil & Environm Engn, Portland, OR 97207 USA.
RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012
FU National Aeronautics and Space Administration under the Ocean Surface
Topography program
FX The satellite data, path delay, and other geophysical corrections used
in this study were extracted from the Radar Altimeter Database System
(Schrama et al. 2000; Scharroo et al. 2013) and from an augmented
version of the Integrated Multi-Mission Ocean Altimeter Database
(http://podaac.jpl.nasa.gov/dataset/MERGED_TP_J1_OSTM_OST_ALL_V2). The
AVISO gridded altimetric data were produced by Ssalto/DUACS with support
from the Centre National d'Etudes Spatiales. This work was funded by the
National Aeronautics and Space Administration under the Ocean Surface
Topography program.
NR 47
TC 6
Z9 6
U1 2
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-3670
EI 1520-0485
J9 J PHYS OCEANOGR
JI J. Phys. Oceanogr.
PD JAN
PY 2016
VL 46
IS 1
BP 3
EP 22
DI 10.1175/JPO-D-15-0065.1
PG 20
WC Oceanography
SC Oceanography
GA DB6LQ
UT WOS:000368626900001
ER
PT J
AU Valdivia-Silva, JE
Karouia, F
Navarro-Gonzalez, R
Mckay, C
AF Valdivia-Silva, Julio E.
Karouia, Fathi
Navarro-Gonzalez, Rafael
Mckay, Christopher
TI MICROORGANISMS, ORGANIC CARBON, AND THEIR RELATIONSHIP WITH OXIDANT
ACTIVITY IN HYPER-ARID MARS-LIKE SOILS: IMPLICATIONS FOR SOIL
HABITABILITY
SO PALAIOS
LA English
DT Article
ID ATACAMA DESERT IMPLICATIONS; COMMUNITY STRUCTURE; BIOMARKER ANALYSIS;
LABELED RELEASE; LIFE; CHILE; ANALOG; COLONIZATION; EXPLORATION; BIOMASS
AB Soil samples from the hyper-arid region in the Atacama Desert in Southern Peru (La Joya Desert) were analyzed for total and labile organic carbon (TOC and LOC), phospholipid fatty acids (PLFA), quantitative real time polymerase chain reaction (qRT-PCR), 4',6-diamidino-2-phenylindole (DAPI)-fluorescent microscopy, culturable microorganisms, and oxidant activity, to understand the relationship between the presence of organic matter and microorganisms in these types of soils. TOC content levels were similar to the labile pool of carbon suggesting the absence of recalcitrant carbon in these soils. LOC ranged between 2 to 60 mg/g of soil. PLFA analysis indicated a maximum of 2.3 x 10(5) cell equivalents/g. Culturing of soil extracts yielded 1.1 x 10(2)-3.7 x 10(3) CFU/g. qRT-PCR showed between 1.0 x 10(2) and 8 x 10(3) cells/g; and DAPI fluorescent staining indicated bacteria counts up to 5 x 10(4) cells/g. Arid and semiarid samples (controls) showed values between 10 7 and 10 11 cells/g with all of the methods used. Importantly, the concentration of microorganisms in hyper-arid soils did not show any correlation with the organic carbon content; however, there was a significant dependence on the oxidant activity present in these soil samples evaluated as the capacity to decompose sodium formate in 10 hours. We suggest that the analysis of oxidant activity could be a useful indicator of the microbial habitability in hyper-arid soils, obviating the need to measure water activity over time. This approach could be useful in astrobiological studies on other worlds.
C1 [Valdivia-Silva, Julio E.; Mckay, Christopher] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Valdivia-Silva, Julio E.] Univ Nacl Ingenieri INICTEL UNI, Inst Nacl Invest & Capacitac Telecomunicac, Lima, Peru.
[Karouia, Fathi] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Karouia, Fathi] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA 94158 USA.
[Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Ciudad Univ, Mexico City 04510, DF, Mexico.
RP Valdivia-Silva, JE (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.; Valdivia-Silva, JE (reprint author), Univ Nacl Ingenieri INICTEL UNI, Inst Nacl Invest & Capacitac Telecomunicac, Lima, Peru.
EM jvaldivia@inictel-uni.edu.pe
RI Gonzalez, Rafael/D-1748-2009
FU National Council of Science and Technology of Mexico (CONACyT) [98466];
Sociedad Cientifica de Astrobiologia del Peru (SCAP); National
Aeronautics and Space Administration, National Autonomous University of
Mexico (DGAPA) [IN106013]
FX This research was supported by grants from the National Aeronautics and
Space Administration, National Autonomous University of Mexico (DGAPA
IN106013), the National Council of Science and Technology of Mexico
(CONACyT 98466), and the Sociedad Cientifica de Astrobiologia del Peru
(SCAP). We thank to Mr. Saul Perez and the two anonymous reviewers for
their comments and suggestions to improve this paper.
NR 61
TC 0
Z9 0
U1 9
U2 26
PU SEPM-SOC SEDIMENTARY GEOLOGY
PI TULSA
PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA
SN 0883-1351
EI 1938-5323
J9 PALAIOS
JI Palaios
PD JAN
PY 2016
VL 31
IS 1
BP 1
EP 9
DI 10.2110/palo.2015.010
PG 9
WC Geology; Paleontology
SC Geology; Paleontology
GA DB4PN
UT WOS:000368495500001
ER
PT S
AU Makino, A
Nelson, D
AF Makino, Alberto
Nelson, Drew
BE Bossuyt, S
Schajer, G
Carpinteri, A
TI Hole Drilling Determination of Residual Stresses Varying Along a Surface
SO RESIDUAL STRESS, THERMOMECHANICS & INFRARED IMAGING, HYBRID TECHNIQUES
AND INVERSE PROBLEMS, VOL 9
SE Conference Proceedings of the Society for Experimental Mechanics Series
LA English
DT Proceedings Paper
CT Annual Conference and Exposition of Society-for-Experimental-Mechanics
on Experimental and Applied Mechanics
CY JUN 08-11, 2015
CL Costa Mesa, CA
SP Soc Experimental Mech
DE Hole-drilling; Residual stress; Optical; Gradient; Interferometric
ID INTERFEROMETRY; GRADIENTS
AB Hole drilling is a widely applied method for determining residual stresses. In numerous cases of practical interest, residual stresses vary significantly along the surface at a location to be drilled. Previous efforts to use strain gages to determine stresses in such cases are briefly reviewed. A computational approach is presented for determining two orthogonal stresses and their surface gradients at a location where stresses can be considered approximately uniform with depth of a drilled hole. The approach is designed for use with optical methods instead of strain gages. Optical interference fringe patterns obtained by holographic interferometry are shown for holes drilled into the side of a beam experiencing elastic bending stresses and associated gradient. Stresses and a gradient determined from fringe patterns are compared with expected values.
C1 [Makino, Alberto] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Makino, Alberto; Nelson, Drew] Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA.
RP Nelson, D (reprint author), Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA.
EM dnelson@stanford.edu
NR 10
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 2191-5644
BN 978-3-319-21765-9; 978-3-319-21764-2
J9 C PROC SOC EXP MECH
PY 2016
BP 347
EP 353
DI 10.1007/978-3-319-21765-9_42
PG 7
WC Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics
SC Engineering; Materials Science; Mechanics
GA BE1SX
UT WOS:000368490000042
ER
PT J
AU Andrews, RJ
Quintana, LM
AF Andrews, Russell J.
Quintana, Leonidas M.
TI Neurosurgical Care for One - Neurosurgical Care for All: Global
Neurosurgical Care Has Global Benefits!
SO WORLD NEUROSURGERY
LA English
DT Editorial Material
DE Cost effectiveness; Global; Innovation; Neurosurgery
ID EDUCATION
C1 [Andrews, Russell J.] NASA, Ames Res Ctr, Nanotechnol & Smart Syst, Moffett Field, CA 94035 USA.
[Quintana, Leonidas M.] Univ Valparaiso, Sch Med, Dept Neurosurg, Valparaiso, Chile.
RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Nanotechnol & Smart Syst, Moffett Field, CA 94035 USA.
EM rja@russelljandrews.org
NR 8
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1878-8750
EI 1878-8769
J9 WORLD NEUROSURG
JI World Neurosurg.
PD JAN
PY 2016
VL 85
BP 22
EP 24
DI 10.1016/j.wneu.2015.08.002
PG 3
WC Clinical Neurology; Surgery
SC Neurosciences & Neurology; Surgery
GA DB0WW
UT WOS:000368229700011
PM 26278867
ER
PT J
AU Megeath, ST
Gutermuth, R
Muzerolle, J
Kryukova, E
Hora, JL
Allen, LE
Flaherty, K
Hartmann, L
Myers, PC
Pipher, JL
Stauffer, J
Young, ET
Fazio, GG
AF Megeath, S. T.
Gutermuth, R.
Muzerolle, J.
Kryukova, E.
Hora, J. L.
Allen, L. E.
Flaherty, K.
Hartmann, L.
Myers, P. C.
Pipher, J. L.
Stauffer, J.
Young, E. T.
Fazio, G. G.
TI THE SPITZER SPACE TELESCOPE SURVEY OF THE ORION A AND B MOLECULAR
CLOUDS. II. THE SPATIAL DISTRIBUTION AND DEMOGRAPHICS OF DUSTY YOUNG
STELLAR OBJECTS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared: stars; ISM: individual objects (Orion A, Orion B); stars:
formation; stars: protostars; stars: variables: T Tauri, Herbig Ae/Be
ID INITIAL MASS FUNCTION; FIELD EXTINCTION MAPS; STAR CLUSTER FORMATION;
X-RAY-EMISSION; NEBULA-CLUSTER; PROTOPLANETARY DISKS; CIRCUMSTELLAR
DISKS; TRAPEZIUM CLUSTER; SOLAR NEIGHBORHOOD; ULTRADEEP PROJECT
AB We analyze the spatial distribution of dusty young stellar objects (YSOs) identified in the Spitzer Survey of the Orion Molecular clouds, augmenting these data with Chandra X-ray observations to correct for incompleteness in dense clustered regions. We also devise a scheme to correct for spatially varying incompleteness when X-ray data are not available. The local surface densities of the YSOs range from 1 pc(-2) to over 10,000 pc(-2), with protostars tending to be in higher density regions. This range of densities is similar to other surveyed molecular clouds with clusters, but broader than clouds without clusters. By identifying clusters and groups as continuous regions with surface densities >= 10 pc(-2), we find that 59% of the YSOs are in the largest cluster, the Orion Nebula Cluster (ONC), while 13% of the YSOs are found in a distributed population. A lower fraction of protostars in the distributed population is evidence that it is somewhat older than the groups and clusters. An examination of the structural properties of the clusters and groups shows that the peak surface densities of the clusters increase approximately linearly with the number of members. Furthermore, all clusters with more than 70 members exhibit asymmetric and/or highly elongated structures. The ONC becomes azimuthally symmetric in the inner 0.1 pc, suggesting that the cluster is only similar to 2 Myr in age. We find that the star formation efficiency (SFE) of the Orion B cloud is unusually low, and that the SFEs of individual groups and clusters are an order of magnitude higher than those of the clouds. Finally, we discuss the relationship between the young low mass stars in the Orion clouds and the Orion OB 1 association, and we determine upper limits to the fraction of disks that may be affected by UV radiation from OB stars or dynamical interactions in dense, clustered regions.
C1 [Megeath, S. T.; Kryukova, E.] Univ Toledo, Dept Phys & Astron, Ritter Astrophs Res Ctr, Toledo, OH 43606 USA.
[Megeath, S. T.] Max Planck Inst Radioastron, Completed Sabbat, D-53121 Bonn, Germany.
[Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hora, J. L.; Myers, P. C.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Flaherty, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hartmann, L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Stauffer, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Young, E. T.] SOFIA Univ Space Res Assoc, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Megeath, ST (reprint author), Univ Toledo, Dept Phys & Astron, Ritter Astrophs Res Ctr, Toledo, OH 43606 USA.
EM megeath@physics.utoledo.edu
FU National Aeronautics and Space Administration; National Science
Foundation; NASA [960541, 960785]; NASA; JPL/Caltech
FX This work benefited immeasurably from discussions with Fred Adams, John
Bally, Cesar Briceno, Neal Evans, Gabor Furesz, Charlie Lada, Pavel
Kroupa, Thomas Henning, Amy Stutz and Scott Wolk. The analysis of the
data would not be possible without the superb support we received from
the staff of the Spitzer Science Center. 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 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 received support through that provided to the IRAC and MIPS
instruments by NASA through contracts 960541 and 960785, respectively,
issued by JPL. Support for this work was also provided by NASA through
awards issued to S. T. M. and JLP by JPL/Caltech. This paper was mostly
completed while S. T. M. was on sabbatical at the Max-Planck-Institut
fur Radioastronomie and further revised while continuing his sabbatical
at the Max-Planck-Institut fur Astronomine. S. T. M. thanks those
institutes for their support.
NR 149
TC 12
Z9 12
U1 0
U2 2
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 JAN
PY 2016
VL 151
IS 1
AR 5
DI 10.3847/0004-6256/151/1/5
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB1EN
UT WOS:000368250900005
ER
PT J
AU Zauderer, BA
Bolatto, AD
Vogel, SN
Carpenter, JM
Perez, LM
Lamb, JW
Woody, DP
Bock, DCJ
Carlstrom, JE
Culverhouse, TL
Curley, R
Leitch, EM
Plambeck, RL
Pound, MW
Marrone, DP
Muchovej, SJ
Mundy, LG
Teng, SH
Teuben, PJ
Volgenau, NH
Wright, MCH
Wu, D
AF Zauderer, B. Ashley
Bolatto, Alberto D.
Vogel, Stuart N.
Carpenter, John M.
Perez, Laura M.
Lamb, James W.
Woody, David P.
Bock, Douglas C. -J.
Carlstrom, John E.
Culverhouse, Thomas L.
Curley, Roger
Leitch, Erik M.
Plambeck, Richard L.
Pound, Marc W.
Marrone, Daniel P.
Muchovej, Stephen J.
Mundy, Lee G.
Teng, Stacy H.
Teuben, Peter J.
Volgenau, Nikolaus H.
Wright, Melvyn C. H.
Wu, Dalton
TI THE CARMA PAIRED ANTENNA CALIBRATION SYSTEM: ATMOSPHERIC PHASE
CORRECTION FOR MILLIMETER WAVE INTERFEROMETRY AND ITS APPLICATION TO
MAPPING THE ULTRALUMINOUS GALAXY ARP 193
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (Arp 193); galaxies: starburst; instrumentation:
interferometers; techniques: interferometric
ID INFRARED GALAXIES; WATER-VAPOR; COMPENSATION EXPERIMENTS;
INTERSTELLAR-MEDIUM; CONVERSION FACTOR; RESOLUTION; SAMPLE; ARRAY;
RADIOMETRY; MONITORS
AB Phase fluctuations introduced by the atmosphere are the main limiting factor in attaining diffraction limited performance in extended interferometric arrays at millimeter and submillimeter wavelengths. We report the results of C-PACS, the Combined Array for Research in Millimeter-Wave Astronomy Paired Antenna Calibration System. We present a systematic study of several hundred test observations taken during the 2009-2010 winter observing season where we utilize CARMA's eight 3.5 m antennas to monitor an atmospheric calibrator while simultaneously acquiring science observations with 6.1 and 10.4 m antennas on baselines ranging from a few hundred meters to similar to 2 km. We find that C-PACS is systematically successful at improving coherence on long baselines under a variety of atmospheric conditions. We find that the angular separation between the atmospheric calibrator and target source is the most important consideration, with consistently successful phase correction at CARMA requiring a suitable calibrator located less than or similar to 6 degrees away from the science target. We show that cloud cover does not affect the success of C-PACS. We demonstrate C-PACS in typical use by applying it to the observations of the nearby very luminous infrared galaxy Arp 193 in (CO)-C-12(2-1) at a linear resolution of approximate to 70 pc (0 ''.12 x 0 ''.18), 3 times better than previously published molecular maps of this galaxy. We resolve the molecular disk rotation kinematics and the molecular gas distribution and measure the gas surface densities and masses on 90 pc scales. We find that molecular gas constitutes similar to 30% of the dynamical mass in the inner 700 pc of this object with a surface density similar to 10(4) M-circle dot pc(-2); we compare these properties to those of the starburst region of NGC 253.
C1 [Zauderer, B. Ashley; Bolatto, Alberto D.; Vogel, Stuart N.; Curley, Roger; Pound, Marc W.; Mundy, Lee G.; Teng, Stacy H.; Teuben, Peter J.; Wu, Dalton] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Zauderer, B. Ashley] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Bolatto, Alberto D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carpenter, John M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Perez, Laura M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Lamb, James W.; Woody, David P.; Leitch, Erik M.; Muchovej, Stephen J.; Volgenau, Nikolaus H.] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
[Bock, Douglas C. -J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Carlstrom, John E.; Culverhouse, Thomas L.; Leitch, Erik M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Plambeck, Richard L.; Wright, Melvyn C. H.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Marrone, Daniel P.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Teng, Stacy H.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zauderer, BA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
FU National Science Foundation; NSF [AST-0838178, AST-1302954,
PHYS-1066293, AST-0955836]; NASA CDDF grant; NSF-Y1 Award; David and
Lucile Packard Foundation; Research Corporation for Science Advancement;
Humboldt Foundation
FX We thank the referee for constructive comments and suggestions. 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. We acknowledge support from NSF AST-0838178. The funds for
the additional hardware for the paired antennas were from a NASA CDDF
grant, an NSF-Y1 Award, and the David and Lucile Packard Foundation.
B.A.Z. wishes to acknowledge the Department of Astronomy at the
University of Maryland, where most of this research was conducted.
B.A.Z. also acknowledges partial support from NSF AST-1302954 (AAPF),
NSF PHYS-1066293, and the hospitality of the Aspen Center for Physics.
A. B. wishes to acknowledge partial support from NSF AST-0955836, a
Cottrell Scholar award from the Research Corporation for Science
Advancement, and the Humboldt Foundation. We thank M. S. Clemens and P.
Alexander for kindly providing their reduced H I data cubes for
comparison and analysis. We acknowledge the input and support in
implementation of this experiment from Owens Valley Radio Observatory
staff Dave Hawkins and Ira Snyder (correlator); Steve Scott, Andy Beard,
and Rick Hobbs (software and computing); Michael Cooper, Ron Lawrence,
Paul Rasmussen, Curt Giovanine, Steve Miller, and Andres Rizo (paired
antenna pad construction and array operations); Brad Wiitala, Michael
Laxen, Russ Keeney, Stan Hudson, and Mark Hodges (receivers and
technical development); John Marzano, Gene Kahn, Mike Virgin, Mary
Daniel, Lori McGraw, Cecil Patrick, and Terry Sepsey (general
operations).
NR 52
TC 0
Z9 0
U1 2
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 JAN
PY 2016
VL 151
IS 1
AR 18
DI 10.3847/0004-6256/151/1/18
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB1EN
UT WOS:000368250900018
ER
PT J
AU David, TJ
Hillenbrand, LA
Cody, AM
Carpenter, JM
Howard, AW
AF David, Trevor J.
Hillenbrand, Lynne A.
Cody, Ann Marie
Carpenter, John M.
Howard, Andrew W.
TI K2 DISCOVERY OF YOUNG ECLIPSING BINARIES IN UPPER SCORPIUS: DIRECT MASS
AND RADIUS DETERMINATIONS FOR THE LOWEST MASS STARS AND INITIAL
CHARACTERIZATION OF AN ECLIPSING BROWN DWARF BINARY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; binaries: spectroscopic; brown dwarfs; stars:
fundamental parameters; stars: low-mass; stars: pre-main sequence
ID PRE-MAIN-SEQUENCE; CENTAURUS OB ASSOCIATION; LIMB-DARKENING
COEFFICIENTS; EVOLUTIONARY MODELS; STELLAR POPULATION; TIME-VARIATION;
SPACED DATA; SPOTS-A; KEPLER; PHOTOMETRY
AB We report the discovery of three low-mass double-lined eclipsing binaries in the pre-main sequence Upper Scorpius association, revealed by K2 photometric monitoring of the region over similar to 78 days. The orbital periods of all three systems are <5 days. We use the K2 photometry plus multiple Keck/HIRES radial velocities (RVs) and spectroscopic flux ratios to determine fundamental stellar parameters for both the primary and secondary components of each system, along with the orbital parameters. We present tentative evidence that EPIC 203868608 is a hierarchical triple system comprised of an eclipsing pair of similar to 25 M-Jup brown dwarfs with a wide M-type companion. If confirmed, it would constitute only the second double-lined eclipsing brown dwarf binary system discovered to date. The double-lined system EPIC 203710387 is composed of nearly identical M4.5-M5 stars with fundamentally determined masses and radii measured to better than 3% precision (M-1= 0.1183 +/- 0.0028M(circle dot), M-2 = 0.1076 +/- 0.0031M(circle dot) and R-1= 0.417 +/- 0.010R(circle dot), R-2 = 0.450 +/- 0.012R(circle dot)) from combination of the light curve and RV time series. These stars have the lowest masses of any stellar mass double-lined eclipsing binary to date. Comparing our derived stellar parameters with evolutionary models, we suggest an age of similar to 10-11 Myr for this system, in contrast to the canonical age of 3-5 Myr for the association. Finally, EPIC 203476597 is a compact single-lined system with a G8-K0 primary and a likely mid-K secondary whose lines are revealed in spectral ratios. Continued measurement of RVs and spectroscopic flux ratios will better constrain fundamental parameters and should elevate the objects to benchmark status. We also present revised parameters for the double-lined eclipsing binary UScoCTIO 5 (M-1= 0.3336 +/- 0.0022M(circle dot), M-2 = 0.3200 +/- 0.0022M(circle dot) and R-1 = 0.862 +/- 0.012, R-2 = 0.852 +/- 0.013R(circle dot)), which are suggestive of a system age younger than previously reported. We discuss the implications of our results on these similar to 0.1-1.5 M stars for pre-main-sequence evolutionary models.
C1 [David, Trevor J.; Hillenbrand, Lynne A.; Carpenter, John M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Cody, Ann Marie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP David, TJ (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA.
EM tjd@astro.caltech.edu
NR 85
TC 16
Z9 16
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 JAN 1
PY 2016
VL 816
IS 1
AR 21
DI 10.3847/0004-637X/816/1/21
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DB0VH
UT WOS:000368225100021
ER
PT J
AU Bustamante, MMC
Roitman, I
Aide, TM
Alencar, A
Anderson, LO
Aragao, L
Asner, GP
Barlow, J
Berenguer, E
Chambers, J
Costa, MH
Fanin, T
Ferreira, LG
Ferreira, J
Keller, M
Magnusson, WE
Morales-Barquero, L
Morton, D
Ometto, JPHB
Palace, M
Peres, CA
Silverio, D
Trumbore, S
Vieira, ICG
AF Bustamante, Mercedes M. C.
Roitman, Iris
Aide, T. . Mitchell
Alencar, Ane
Anderson, Liana O.
Aragao, Luiz
Asner, Gregory P.
Barlow, Jos
Berenguer, Erika
Chambers, Jeffrey
Costa, Marcos H.
Fanin, Thierry
Ferreira, Laerte G.
Ferreira, Joice
Keller, Michael
Magnusson, William E.
Morales-Barquero, Lucia
Morton, Douglas
Ometto, Jean P. H. B.
Palace, Michael
Peres, Carlos A.
Silverio, Divino
Trumbore, Susan
Vieira, Ima C. G.
TI Toward an integrated monitoring framework to assess the effects of
tropical forest degradation and recovery on carbon stocks and
biodiversity
SO GLOBAL CHANGE BIOLOGY
LA English
DT Review
DE carbon emissions; ecosystem modeling; field inventories; forest
dynamics; remote sensing
ID MEDIATED SEED DISPERSAL; BRAZILIAN AMAZON; TREE MORTALITY; CANOPY
DAMAGE; FIRE BEHAVIOR; DENSITY MAPS; BIOMASS; EMISSIONS; DEFORESTATION;
STORAGE
AB Tropical forests harbor a significant portion of global biodiversity and are a critical component of the climate system. Reducing deforestation and forest degradation contributes to global climate-change mitigation efforts, yet emissions and removals from forest dynamics are still poorly quantified. We reviewed the main challenges to estimate changes in carbon stocks and biodiversity due to degradation and recovery of tropical forests, focusing on three main areas: (1) the combination of field surveys and remote sensing; (2) evaluation of biodiversity and carbon values under a unified strategy; and (3) research efforts needed to understand and quantify forest degradation and recovery. The improvement of models and estimates of changes of forest carbon can foster process-oriented monitoring of forest dynamics, including different variables and using spatially explicit algorithms that account for regional and local differences, such as variation in climate, soil, nutrient content, topography, biodiversity, disturbance history, recovery pathways, and socioeconomic factors. Generating the data for these models requires affordable large-scale remote-sensing tools associated with a robust network of field plots that can generate spatially explicit information on a range of variables through time. By combining ecosystem models, multiscale remote sensing, and networks of field plots, we will be able to evaluate forest degradation and recovery and their interactions with biodiversity and carbon cycling. Improving monitoring strategies will allow a better understanding of the role of forest dynamics in climate-change mitigation, adaptation, and carbon cycle feedbacks, thereby reducing uncertainties in models of the key processes in the carbon cycle, including their impacts on biodiversity, which are fundamental to support forest governance policies, such as Reducing Emissions from Deforestation and Forest Degradation.
C1 [Bustamante, Mercedes M. C.; Roitman, Iris; Silverio, Divino] Univ Brasilia, Dept Ecol, BR-70910900 Brasilia, DF, Brazil.
[Aide, T. . Mitchell] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA.
[Alencar, Ane] Amazon Environm Res Inst IPAM, Brasilia, DF, Brazil.
[Anderson, Liana O.] Natl Ctr Monitoring & Early Warning Nat Disasters, BR-12247016 Sao Jose Dos Campos, SP, Brazil.
[Anderson, Liana O.] Univ Oxford, Environm Change Inst, Oxford OX1 3QY, England.
[Anderson, Liana O.; Aragao, Luiz] Inst Nacl Pesquisas Espaciais, BR-12247016 Sao Jose Dos Campos, SP, Brazil.
[Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Barlow, Jos; Berenguer, Erika] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Barlow, Jos; Vieira, Ima C. G.] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil.
[Chambers, Jeffrey] Univ Calif Berkeley, Dept Geog, Berkeley, CA 94720 USA.
[Costa, Marcos H.] Univ Fed Vicosa, Dept Agr Engn, BR-36570900 Vicosa, MG, Brazil.
[Fanin, Thierry] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands.
[Ferreira, Laerte G.] Univ Fed Goias, Inst Estudo Socioambientais, Goiania, Go, Brazil.
[Ferreira, Joice] Embrapa Amazonia Oriental, BR-66017970 Belem, Para, Brazil.
[Keller, Michael] US Forest Serv, USDA, Int Inst Trop Forestry, San Juan, PR USA.
[Keller, Michael] EMBRAPA Monitoramento Satelite, Campinas, SP, Brazil.
[Magnusson, William E.] Inst Nacl de Pesquisas da Amazonia, BR-69067971 Manaus, Amazonas, Brazil.
[Morales-Barquero, Lucia] Bangor Univ, Coll Nat Sci, Sch Environm Nat Resources & Geog, Bangor LL57 2UW, Gwynedd, Wales.
[Morton, Douglas] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Ometto, Jean P. H. B.] Natl Inst Space Res INPE, Earth Syst Sci Ctr CCST, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Palace, Michael] UNH, Inst Study Earth Oceans & Space, Earth Syst Res Ctr, Norwich, Norfolk, England.
[Peres, Carlos A.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Trumbore, Susan] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
RP Bustamante, MMC (reprint author), Univ Brasilia, Dept Ecol, BR-70910900 Brasilia, DF, Brazil.
EM mercedes@unb.br
RI Morton, Douglas/D-5044-2012; Keller, Michael/A-8976-2012; Barlow,
Jos/E-7861-2014; Peres, Carlos/B-1276-2013; Chambers,
Jeffrey/J-9021-2014; Silverio, Divino Vicente/G-1154-2012; Bustamante,
Mercedes/H-7597-2015;
OI Keller, Michael/0000-0002-0253-3359; Peres, Carlos/0000-0002-1588-8765;
Chambers, Jeffrey/0000-0003-3983-7847; Silverio, Divino
Vicente/0000-0003-1642-9496; Bustamante, Mercedes/0000-0003-1008-452X;
Berenguer, Erika/0000-0001-8157-8792; Roitman, Iris/0000-0002-1698-1777
FU Climate Land Use Alliance; Science Without Borders Program (CNPq); Rede
Clima of Brazilian Ministry of Science, Technology and Innovation; NERC
[NE/K016431/1]
FX This document is based on the discussions held during the Workshop on
Monitoring Forest Dynamics: carbon stocks, greenhouse gas fluxes, and
biodiversity, in Brasilia, Brazil (September 2-4, 2014) financed by
Climate Land Use Alliance. Susan Trumbore and Douglas Morton acknowledge
the financial support from the Science Without Borders Program (CNPq).
Mercedes Bustamante and Iris Roitman acknowledge the financial support
of the Rede Clima of Brazilian Ministry of Science, Technology and
Innovation. J.B. and E.B. were supported by a grant from the NERC
(NE/K016431/1). The authors are grateful to TobyGardner for valuable
comments on previous version of this article.
NR 131
TC 9
Z9 9
U1 31
U2 109
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 JAN
PY 2016
VL 22
IS 1
BP 92
EP 109
DI 10.1111/gcb.13087
PG 18
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA DA7KL
UT WOS:000367982900007
PM 26390852
ER
PT J
AU Ye, Y
Yu, B
Tang, A
Drouin, B
Gu, QJ
AF Ye, Yu
Yu, Bo
Tang, Adrian
Drouin, Brian
Gu, Qun Jane
TI A High Efficiency E-Band CMOS Frequency Doubler With a Compensated
Transformer-Based Balun for Matching Enhancement
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Broadband; frequency doubler; high efficiency; push-push; transformer
AB This letter presents a broadband high efficiency frequency doubler based on a new and effective compensation technique. A transformer based input balun achieves good balanced performance and input matching by the newly invented central capacitor based compensation technique. It demonstrates a peak conversion gain (CG) of -2.5 dB and peak efficiency of 9.7% with a saturated output power of 2.5 dBm at 74 GHz. The doubler exhibits a 3 dB CG bandwidth of 28 GHz from 62 to 90 GHz. The fundamental rejection is larger than 20 dB. The doubler is fabricated in a 65 nm CMOS technology with chip area of 0.6 x 0.45 mm(2) and consumes 9-14 mW power.
C1 [Ye, Yu; Yu, Bo; Tang, Adrian; Gu, Qun Jane] Univ Calif Davis, High Speed Integrated Circuits & Syst Lab, Davis, CA 95616 USA.
[Tang, Adrian; Drouin, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ye, Y (reprint author), Univ Calif Davis, High Speed Integrated Circuits & Syst Lab, Davis, CA 95616 USA.
EM yuye@ucdavis.edu; jgu@ucdavis.edu
FU National Aeronautics and Space Administration through the Planetary
Science Division PICASSO program [NNN13D485T]
FX This work was supported by the National Aeronautics and Space
Administration under Grant NNN13D485T issued through the Planetary
Science Division PICASSO program.
NR 7
TC 4
Z9 4
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD JAN
PY 2016
VL 26
IS 1
BP 40
EP 42
DI 10.1109/LMWC.2015.2505617
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA DA6XU
UT WOS:000367949900014
ER
PT J
AU Ponchak, GE
AF Ponchak, George E.
TI Slotline Switch Based on a Lattice Circuit
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Lattice circuit; pin diode; slotline; switch
AB Slotline switches are required for many slotline applications, such as tunable slot antennas and slotline antenna feed networks. The current practice is to place a pin diode or MEMS device across the slot to create a short circuit when the switch is in the OFF state. In this letter, a slotline short circuit series stub is incorporated into a lattice circuit to achieve a switch with a theoretical 0 dB insertion loss, infinite isolation and infinite return loss over a narrow bandwidth. Measured results demonstrate a near zero insertion loss, approximately 40 dB of isolation and greater than 15 dB return loss at 4.25 GHz, with an approximate 40% bandwidth defined by return loss and isolation greater than 10 dB.
C1 [Ponchak, George E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM george.ponchak@ieee.org
NR 10
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD JAN
PY 2016
VL 26
IS 1
BP 43
EP 45
DI 10.1109/LMWC.2015.2505639
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA DA6XU
UT WOS:000367949900015
ER
PT J
AU Masnovi, J
Duffy, NV
Fanwick, PE
Hepp, AF
AF Masnovi, John
Duffy, Norman V.
Fanwick, Philip E.
Hepp, Aloysius F.
TI Structural characterization and preliminary decomposition study of four
unsymmetrically substituted nickel dithiocarbamate complexes
SO JOURNAL OF COORDINATION CHEMISTRY
LA English
DT Article
DE Nickel dithiocarbamate; X-ray diffraction; triphenylphosphine; crystal
structures; thermogravimetric analysis
ID SINGLE-SOURCE PRECURSOR; SULFIDE THIN-FILMS; CRYSTAL-STRUCTURE;
COORDINATION SPHERE; DNA-BINDING; NI(II); DEPOSITION;
TRIPHENYLPHOSPHINE; NANOPARTICLES; LIGANDS
AB Single-crystal X-ray structures of four nickel dithiocarbamate complexes, the homoleptic mixed-organic bis-dithiocarbamates Ni[S2CN(isopropyl)(benzyl)](2), Ni[S2CN(ethyl)(n-butyl)](2), and Ni[S2CN(phenyl)(benzyl)](2), as well as the heteroleptic mixed-ligand complex NiCl[P(phenyl)(3)][(S2CN(phenyl)(benzyl)], were determined. A slightly distorted square-planar nickel coordination environment was observed for all four complexes. The organic residues adopt conformations to minimize steric interactions. Steric effects also may determine puckering, if any, about the nickel and nitrogen atoms, both of which are planar or nearly so. A trans-influence affects the Ni-S bond distances. Nitrogens interact with the CS2 carbons with a bond order near two; the other substituents on nitrogen display transoid conformations. There are no strong intermolecular interactions, consistent with prior observations of the volatility of nickel dithiocarbamate complexes. A preliminary thermolysis study of the homoleptic species results in production of 1:1 nickel sulfide phases, indicating the potential utility of these species as single-source precursors.
[GRAPHICS]
.
C1 [Masnovi, John] Cleveland State Univ, Dept Chem, Cleveland, OH 44115 USA.
[Duffy, Norman V.] Wheeling Jesuit Univ, Dept Chem, Wheeling, WV USA.
[Fanwick, Philip E.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Hepp, Aloysius F.] NASA Glenn Res Ctr, Photovolta & Elect Syst Branch, Cleveland, OH 44135 USA.
RP Hepp, AF (reprint author), NASA Glenn Res Ctr, Photovolta & Elect Syst Branch, Cleveland, OH 44135 USA.
EM Aloysius.F.Hepp@nasa.gov
FU NASA GRC Faculty Fellowship Program
FX Work at NASA Glenn Research Center was supported by several internal
research and development programs (A.F. Hepp and D. Ogrin) and the NASA
GRC Faculty Fellowship Program (for J. Masnovi).
NR 67
TC 1
Z9 1
U1 8
U2 15
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0095-8972
EI 1029-0389
J9 J COORD CHEM
JI J. Coord. Chem.
PY 2016
VL 69
IS 1
BP 90
EP 102
DI 10.1080/00958972.2015.1107904
PG 13
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA DA8VP
UT WOS:000368084900009
ER
PT J
AU Suhir, E
Ghaffarian, R
Nicolics, J
AF Suhir, E.
Ghaffarian, R.
Nicolics, J.
TI Could thermal stresses in a BGA/CGA-system be evaluated from a model
intended for a homogeneously bonded assembly?
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID BIMETAL THERMOSTATS; BONDING LAYER; CCGA
AB An analytical stress model is developed for the evaluation of thermal stresses in an inhomogeneously bonded assembly of the ball-grid-array (BGA) or column grid array (CGA) type. It is shown that one can get away with employing a simpler model intended for an assembly with a homogeneous bond, if the gaps between the supports (BGA balls or CGA columns) are small, so that the ratio of the pitch p (the distance between the joint centers) to the joint widths 2l is below 5, and the product kl of the parameter k of the interfacial shearing stress and half the assembly length l in the equivalent homogeneously bonded assembly is above 2.5. This is indeed the case for actual BGA and CGA systems. This finding can be used also in other areas of engineering, such as, say, mechanical or structural, when there is an intent to simplify the calculations by replacing a model for beams on separate supports by using a model intended for a beam on a continuous elastic foundation.
C1 [Suhir, E.] Portland State Univ, Portland, OR 97207 USA.
[Suhir, E.] ERS Co, Los Altos, CA 94024 USA.
[Ghaffarian, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suhir, E.; Nicolics, J.] Vienna Univ Technol, A-1040 Vienna, Austria.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.
EM suhire@aol.com; reza.ghaffarian@jpl.nasa.gov;
Johann.Nicolics@tuwien.ac.at
NR 24
TC 6
Z9 6
U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD JAN
PY 2016
VL 27
IS 1
BP 570
EP 579
DI 10.1007/s10854-015-3790-9
PG 10
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA DA8KX
UT WOS:000368054600076
ER
PT J
AU Richardson, ND
Moffat, AFJ
Maltais-Tariant, R
Pablo, H
Gies, DR
Saio, H
St-Louis, N
Schaefer, G
Miroshnichenko, AS
Farrington, C
Aldoretta, EJ
Artigau, E
Boyajian, TS
Gordon, K
Jones, J
Matson, R
McAlister, HA
O'Brien, D
Raghavan, D
Ramiaramanantsoa, T
Ridgway, ST
Scott, N
Sturmann, J
Sturmann, L
ten Brummelaar, T
Thomas, JD
Turner, N
Vargas, N
Zharikov, S
Matthews, J
Cameron, C
Guenther, D
Kuschnig, R
Rowe, J
Rucinski, S
Sasselov, D
Weiss, W
AF Richardson, Noel D.
Moffat, Anthony F. J.
Maltais-Tariant, Raphael
Pablo, Herbert
Gies, Douglas R.
Saio, Hideyuki
St-Louis, Nicole
Schaefer, Gail
Miroshnichenko, Anatoly S.
Farrington, Chris
Aldoretta, Emily J.
Artigau, Etienne
Boyajian, Tabetha S.
Gordon, Kathryn
Jones, Jeremy
Matson, Rachel
McAlister, Harold A.
O'Brien, David
Raghavan, Deepak
Ramiaramanantsoa, Tahina
Ridgway, Stephen T.
Scott, Nic
Sturmann, Judit
Sturmann, Laszlo
ten Brummelaar, Theo
Thomas, Joshua D.
Turner, Nils
Vargas, Norm
Zharikov, Sergey
Matthews, Jaymie
Cameron, Chris
Guenther, David
Kuschnig, Rainer
Rowe, Jason
Rucinski, Slavek
Sasselov, Dimitar
Weiss, Werner
TI Spectroscopy, MOST photometry, and interferometry of MWC 314: is it an
LBV or an interacting binary?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; stars: early-type; stars: individual: MWC 314; stars:
massloss; stars: variables: S Doradus; stars: winds, outflows
ID SECULAR ORBITAL EVOLUTION; CHARA ARRAY; MASSIVE STARS; P-CYGNI; SYSTEM;
SUPERGIANTS; VARIABLES; SPECTROPHOTOMETRY; SPECTROMETER; VARIABILITY
AB MWC 314 is a bright candidate luminous blue variable (LBV) that resides in a fairly close binary system, with an orbital period of 60.753 +/- 0.003 d. We observed MWC 314 with a combination of optical spectroscopy, broad-band ground-and space-based photometry, as well as with long baseline, near-infrared interferometry. We have revised the single-lined spectroscopic orbit and explored the photometric variability. The orbital light curve displays two minima each orbit that can be partially explained in terms of the tidal distortion of the primary that occurs around the time of periastron. The emission lines in the system are often double-peaked and stationary in their kinematics, indicative of a circumbinary disc. We find that the stellar wind or circumbinary disc is partially resolved in the K' -band with the longest baselines of the CHARA Array. From this analysis, we provide a simple, qualitative model in an attempt to explain the observations. From the assumption of Roche Lobe overflow and tidal synchronization at periastron, we estimate the component masses to be M-1 approximate to 5M(circle dot) and M-2 approximate to 15M(circle dot), which indicates a mass of the LBV that is extremely low. In addition to the orbital modulation, we discovered two pulsational modes with the MOST satellite. These modes are easily supported by a low-mass hydrogen-poor star, but cannot be easily supported by a star with the parameters of an LBV. The combination of these results provides evidence that the primary star was likely never a normal LBV, but rather is the product of binary interactions. As such, this system presents opportunities for studying mass-transfer and binary evolution with many observational techniques.
C1 [Richardson, Noel D.; Moffat, Anthony F. J.; Maltais-Tariant, Raphael; Pablo, Herbert; St-Louis, Nicole; Aldoretta, Emily J.; Artigau, Etienne; Ramiaramanantsoa, Tahina] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Richardson, Noel D.; Moffat, Anthony F. J.; Maltais-Tariant, Raphael; Pablo, Herbert; St-Louis, Nicole; Aldoretta, Emily J.; Artigau, Etienne; Ramiaramanantsoa, Tahina] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada.
[Gies, Douglas R.; Gordon, Kathryn; Jones, Jeremy; Matson, Rachel; McAlister, Harold A.; Raghavan, Deepak] Georgia State Univ, Dept Phys & Astron, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Saio, Hideyuki] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan.
[Schaefer, Gail; Farrington, Chris; Scott, Nic; Sturmann, Judit; Sturmann, Laszlo; ten Brummelaar, Theo; Turner, Nils; Vargas, Norm] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA.
[Miroshnichenko, Anatoly S.] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 USA.
[Boyajian, Tabetha S.] Yale Univ, New Haven, CT 06520 USA.
[O'Brien, David] Max Planck Inst Radio Astron, D-53010 Bonn, Germany.
[Ridgway, Stephen T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Thomas, Joshua D.] Clarkson Univ, Dept Phys, Potsdam, NY 13699 USA.
[Zharikov, Sergey] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, BC, Mexico.
[Matthews, Jaymie; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Australia.
[Guenther, David] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Rowe, Jason] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rucinski, Slavek] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Richardson, ND (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
EM richardson@astro.umontreal.ca
OI Richardson, Noel/0000-0002-2806-9339
FU CRAQ (Centre de Recherche en Astrophysique du Quebec); NSERC (Canada);
FRQNT (Quebec); NSF [AST-1411654]; DGAPA/PAPIIT project [IN100614]; NASA
[ADAP12-0172]; NOAO Programs [2009B-0153, 2012A-0216]; Robert Martin
Ayers Sciences Fund; GSU College of Arts and Sciences; National Science
Foundation [AST-0606958, AST-0908253, AST-1211129]; W. M. Keck
Foundation; NASA Exoplanet Science Institute; Georgia State University;
David and Lucile Packard Foundation
FX We thank the anonymous referee for helping the analysis and presentation
of this paper. We are grateful to Fred Walter (Stony Brook University)
for his scheduling of spectroscopic observations with the CTIO 1.5 m, to
the CTIO SMARTS staff for queue observing support, and to Todd Henry
(Georgia State University) for assistance in scheduling the initial
observations with the SMARTS echelle spectrograph. We are also grateful
to John Monnier (Univ. of Michigan) for contributions to data reduction
and analysis. We thank Pierre-Luc Levesque, Bernard Malenfant, Ghislain
Turcotte, and Philippe Vallee for their assistance in obtaining data at
the OMM. Some spectra with the CTIO 1.5 m were obtained through the NOAO
Programs 2009B-0153 and 2012A-0216. This work was partially based on
observations obtained at the 2.1-m Otto Struve and 2.7-m Harlan. J.
Smith telescopes of the McDonald Observatory of the University of Texas
at Austin. This work was also based partially on observations obtained
at the Mercator telescopes and HERMES spectrograph of the Instituto de
Astrofisica de Canarias. This research was made possible through the use
of the APASS, funded by the Robert Martin Ayers Sciences Fund.
Operational funding for the CHARA Array is provided by the GSU College
of Arts and Sciences, by the National Science Foundation through grants
AST-0606958, AST-0908253, and AST-1211129, by the W. M. Keck Foundation,
and by the NASA Exoplanet Science Institute. We thank the Mount Wilson
Institute for providing infrastructure support at Mount Wilson
Observatory. The CHARA Array, operated by Georgia State University, was
built with funding provided by the National Science Foundation, Georgia
State University, the W. M. Keck Foundation, and the David and Lucile
Packard Foundation. This research has made use of the SIMBAD data base,
operated at CDS, Strasbourg, France.; NDR is grateful for his CRAQ
(Centre de Recherche en Astrophysique du Quebec) postdoctoral
fellowship. AFJM and NSL are grateful for financial support from NSERC
(Canada) and FRQNT (Quebec). DRG and GS acknowledge support from NSF
grant AST-1411654. AM and SZ acknowledge support from DGAPA/PAPIIT
project IN100614. TSB acknowledges support provided through NASA grant
ADAP12-0172.
NR 68
TC 3
Z9 3
U1 2
U2 2
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 1
PY 2016
VL 455
IS 1
BP 244
EP 257
DI 10.1093/mnras/stv2291
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900042
ER
PT J
AU Helgason, K
Ricotti, M
Kashlinsky, A
Bromm, V
AF Helgason, K.
Ricotti, M.
Kashlinsky, A.
Bromm, V.
TI On the physical requirements for a pre-reionization origin of the
unresolved near-infrared background
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE dark ages, reionization, first stars; diffuse radiation; early universe;
galaxies: high-redshift
ID POPULATION-III STARS; MASSIVE BLACK-HOLES; ULTRAVIOLET LUMINOSITY
FUNCTION; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; LARGE-SCALE
STRUCTURE; DARK-MATTER HALOES; ULTRA DEEP FIELD; 1ST GALAXIES; FORMATION
HISTORIES
AB The study of the cosmic near-infrared background (CIB) light after subtraction of resolved sources can push the limits of current observations and yield information on galaxies and quasars in the early universe. Spatial fluctuations of the CIB exhibit a clustering excess at angular scales similar to 1 degrees whose origin has not been conclusively identified, but disentangling the relative contribution from low-and high-redshift sources is not trivial. We explore the likelihood that this signal is dominated by emission from galaxies and accreting black holes (BHs) in the early Universe. We find that, the measured fluctuation signal is too large to be produced by galaxies at redshifts z > 8, which only contribute similar to 0.01-0.05 nW m(-2) sr(-1) to the CIB. Additionally, if the first small mass galaxies have a normal initial mass function, the light of their ageing stars (fossils) integrated over cosmic time contributes a comparable amount to the CIB as their pre-reionization progenitors. In order to produce the observed level of CIB fluctuation without violating constraints from galaxy counts and the electron optical depth of the IGM, minihaloes at z > 12 must form preferably top-heavy stars with efficiency f(*) greater than or similar to 0.1 and at the same time maintain a very low escape fraction of ionizing radiation, f(esc) < 0.1 per cent. If instead the CIB fluctuations are produced by high-z BHs, one requires vigorous accretion in the early universe reaching rho(acc) greater than or similar to 10(5) M-circle dot Mpc(-3) by z similar or equal to 10. This growth must stop by z similar to 6 and be significantly obscured not to overproduce the soft cosmic X-ray background and its observed coherence with the CIB. We therefore find the range of suitable high-z explanations to be narrow, but could possibly be widened by including additional physics and evolution at those epochs.
C1 [Helgason, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Ricotti, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] SSAI, Lanham, MD 20706 USA.
[Bromm, V.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Helgason, K (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
EM kari@mpa-garching.mpg.de
FU European Unions Seventh Framework Programme [628319-CIBorigins]; NASA
Headquarters under the NESSF Program [NNX11AO05H]; NSF CDI-typeII grant
[CMMI1125285]; Theoretical and Computational Astrophysics Network (TCAN)
grant [AST1333514]; NASA [NNN12AA01C]; NSF [AST-1413501]
FX We thank B. Yue, A. Ferrara, N. Cappelluti and E. Komatsu for useful
discussions. KH was supported by the European Unions Seventh Framework
Programme (FP7-PEOPLE-2013-IFF) under grant agreement number
628319-CIBorigins, and by NASA Headquarters under the NESSF Program
Grant - NNX11AO05H. MR acknowledges support from NSF CDI-typeII grant
CMMI1125285 and the Theoretical and Computational Astrophysics Network
(TCAN) grant AST1333514. AK acknowledges NASA's support for the Euclid
LIBRAE project NNN12AA01C. VB was supported by NSF grant AST-1413501.
NR 112
TC 5
Z9 5
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 1
PY 2016
VL 455
IS 1
BP 282
EP 294
DI 10.1093/mnras/stv2209
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900045
ER
PT J
AU Lipunov, VM
Gorosabel, J
Pruzhinskaya, MV
Postigo, AD
Pelassa, V
Tsvetkova, AE
Sokolov, IV
Kann, DA
Xu, D
Gorbovskoy, ES
Krushinski, VV
Kornilov, VG
Balanutsa, PV
Boronina, SV
Budnev, NM
Cano, Z
Castro-Tirado, AJ
Chazov, VV
Connaughton, V
Delvaux, C
Frederiks, DD
Fynbo, JFU
Gabovich, AV
Goldstein, A
Greiner, J
Gress, OA
Ivanov, KI
Jakobsson, P
Klose, S
Knust, F
Komarova, VN
Konstantinov, E
Krylov, AV
Kuvshinov, DA
Kuznetsov, AS
Lipunova, GV
Moskvitin, AS
Pal'shin, VD
Pandey, SB
Poleshchuk, VA
Schmidl, S
Sergienko, YP
Sinyakov, EV
Schulze, S
Sokolov, VV
Sokolova, TN
Sparre, M
Thone, CC
Tlatov, AG
Tyurina, NV
Ulanov, MV
Yazev, SA
Yurkov, VV
AF Lipunov, V. M.
Gorosabel, J.
Pruzhinskaya, M. V.
de Ugarte Postigo, A.
Pelassa, V.
Tsvetkova, A. E.
Sokolov, I. V.
Kann, D. A.
Xu, Dong
Gorbovskoy, E. S.
Krushinski, V. V.
Kornilov, V. G.
Balanutsa, P. V.
Boronina, S. V.
Budnev, N. M.
Cano, Z.
Castro-Tirado, A. J.
Chazov, V. V.
Connaughton, V.
Delvaux, C.
Frederiks, D. D.
Fynbo, J. F. U.
Gabovich, A. V.
Goldstein, A.
Greiner, J.
Gress, O. A.
Ivanov, K. I.
Jakobsson, P.
Klose, S.
Knust, F.
Komarova, V. N.
Konstantinov, E.
Krylov, A. V.
Kuvshinov, D. A.
Kuznetsov, A. S.
Lipunova, G. V.
Moskvitin, A. S.
Pal'shin, V. D.
Pandey, S. B.
Poleshchuk, V. A.
Schmidl, S.
Sergienko, Yu. P.
Sinyakov, E. V.
Schulze, S.
Sokolov, V. V.
Sokolova, T. N.
Sparre, M.
Thoene, C. C.
Tlatov, A. G.
Tyurina, N. V.
Ulanov, M. V.
Yazev, S. A.
Yurkov, V. V.
TI The optical identification of events with poorly defined locations: the
case of the Fermi GBM GRB 140801A
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE acceleration of particles; black hole physics; magnetic field;
gamma-ray: general; X-ray: general
ID GAMMA-RAY BURSTS; COMPLETE SAMPLE; LIGHT CURVES; AFTERGLOWS; SPECTRA;
MASTER; TELESCOPE; LUMINOSITY; CATALOG; NETWORK
AB We report the early discovery of the optical afterglow of gamma-ray burst (GRB) 140801A in the 137 deg(2) 3-sigma error-box of the Fermi Gamma-ray Burst Monitor (GBM). MASTER is the only observatory that automatically reacts to all Fermi alerts. GRB 140801A is one of the few GRBs whose optical counterpart was discovered solely from its GBM localization. The optical afterglow of GRB 140801A was found by MASTER Global Robotic Net 53 s after receiving the alert, making it the fastest optical detection of a GRB from a GBM error-box. Spectroscopy obtained with the 10.4-m Gran Telescopio Canarias and the 6-m Big Telescope Alt-azimuth of the Special Astrophysical Observatory of the Russian Academy of Sciences reveals a redshift of z = 1.32. We performed optical and near-infrared photometry of GRB 140801A using different telescopes with apertures ranging from 0.4 to 10.4 m. GRB 140801A is a typical burst in many ways. The rest-frame bolometric isotropic energy release and peak energy of the burst are E-iso = 5.54(-0.24)(+0.26) x 10(52) erg and E-p,E- rest similar or equal to 280 keV, respectively, which is consistent with the Amati relation. The absence of a jet break in the optical light curve provides a lower limit on the half-opening angle of the jet theta = 6 degrees.1. The observed E-peak is consistent with the limit derived from the Ghirlanda relation. The joint Fermi GBM and Konus-Wind analysis show that GRB 140801A could belong to the class of intermediate duration. The rapid detection of the optical counterpart of GRB 140801A is especially important regarding the upcoming experiments with large coordinate error-box areas.
C1 [Lipunov, V. M.; Kornilov, V. G.; Kuvshinov, D. A.] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia.
[Lipunov, V. M.; Pruzhinskaya, M. V.; Gorbovskoy, E. S.; Kornilov, V. G.; Balanutsa, P. V.; Chazov, V. V.; Krylov, A. V.; Kuvshinov, D. A.; Kuznetsov, A. S.; Lipunova, G. V.; Tyurina, N. V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119234, Russia.
[Lipunov, V. M.; Gorbovskoy, E. S.] Moscow MV Lomonosov State Univ, Extreme Universe Lab, Inst Nucl Phys, Moscow 119991, Russia.
[Gorosabel, J.; de Ugarte Postigo, A.; Castro-Tirado, A. J.; Thoene, C. C.] Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Gorosabel, J.] Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain.
[Gorosabel, J.] Univ Basque Country, Grp Ciencias Planetarias, ETS Ingn, Dept Fis Aplicada 1,UPV EHU IAA CSIC,Unidad Asoci, E-48013 Bilbao, Spain.
[de Ugarte Postigo, A.; Xu, Dong; Fynbo, J. F. U.; Sparre, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Pelassa, V.; Connaughton, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Pelassa, V.; Pal'shin, V. D.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Tsvetkova, A. E.; Frederiks, D. D.; Ulanov, M. V.] Ioffe Inst, St Petersburg 194021, Russia.
[Sokolov, I. V.] Russian AS, Terskol Branch, Inst Astron, Tyrnyauz 361623, Russia.
[Kann, D. A.; Klose, S.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Xu, Dong] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Xu, Dong] Chinese Acad Sci, Natl Astron Observ, Key Lab Space Astron & Technol, Beijing 100012, Peoples R China.
[Krushinski, V. V.] Ural Fed Univ, Kourovka Astron Observ, Ekaterinburg 620000, Russia.
[Boronina, S. V.] St Petersburg State Univ, St Petersburg 199034, Russia.
[Budnev, N. M.; Gress, O. A.; Ivanov, K. I.; Konstantinov, E.; Poleshchuk, V. A.; Yazev, S. A.] Irkutsk State Univ, Inst Appl Phys, Irkutsk 664003, Russia.
[Cano, Z.; Jakobsson, P.] Univ Iceland, Ctr Astrophys & Cosmol, Inst Sci, IS-107 Reykjavik, Iceland.
[Castro-Tirado, A. J.] Univ Malaga, Unidad Asociada, Dept Ingn Sistemas & Automiat, E-29071 Malaga, Spain.
[Connaughton, V.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Delvaux, C.; Greiner, J.; Knust, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gabovich, A. V.; Sergienko, Yu. P.; Sinyakov, E. V.; Yurkov, V. V.] Blagoveschensk State Pedag Univ, Blagoveshchensk 675000, Amur Region, Russia.
[Goldstein, A.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Greiner, J.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany.
[Komarova, V. N.; Sokolov, V. V.; Sokolova, T. N.] Russian AS, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia.
[Pandey, S. B.] Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India.
[Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile.
[Schulze, S.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Tlatov, A. G.] RAS, Main Pulkovo Observ, Kislovodsk Solar Stn, Kislovodsk 357700, Russia.
[Ulanov, M. V.] Peter Great St Petersburg Polytech Univ, St Petersburg 195251, Russia.
RP Lipunov, VM (reprint author), Moscow MV Lomonosov State Univ, Fac Phys, GSP 1, Moscow 119991, Russia.
EM lipunov2007@gmail.com
RI Ivanov, Kirill/O-9236-2015; Gorbovskoy, Evgeny/O-8845-2015;
OI Gorbovskoy, Evgeny/0000-0002-4368-9237; de Ugarte Postigo,
Antonio/0000-0001-7717-5085; Frederiks, Dmitry/0000-0002-1153-6340;
Sparre, Martin/0000-0002-9735-3851; Thone,
Christina/0000-0002-7978-7648; Schulze, Steve/0000-0001-6797-1889
FU Development Programme of Lomonosov Moscow State University; RFBR
[15-02-07875, 14-32-50547]; Russian Federation Ministry of Education and
Science [14.B25.31.0010, 2014/51, 1366]; NASA; Russian Foundation of
Fundamental Research [RFBR 14-02-31546, 14-02-91172]; Russian Space
Agency, RFBR [15-02-00532a, 13-02-12017 ofi-m]; DFG [HA 1850/28-1, Kl
766/16-1, 766/16-3]; Spanish Ministry Grant [AYA 2012-39727-C03-01];
EXTraS from European Union [607452]; Thuringer Ministerium fur Bildung,
Wissenschaft und Kultur [FKZ 12010-514]; Division of Physics, Russian
Academy of Sciences [OFN-17]; Russian Federation [MK-1699.2014.2];
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]; [3.615.2014/K]
FX MASTER Global Robotic Net is supported in part by the Development
Programme of Lomonosov Moscow State University. This work was also
supported in part by RFBR 15-02-07875 grant.; This work is also
partially supported by the Russian Federation Ministry of Education and
Science (agreement 14.B25.31.0010 and government assignment 2014/51,
project 1366) and by state order No. 3.615.2014/K in relation to
scientific activity (design part).; The Fermi GBM collaboration
acknowledges support for GBM development, operations, and data analysis
from NASA in the U.S.A and BMWi/DLR in Germany. AG is supported by an
appointment to the NASA Postdoctoral Program at MSFC, administered by
Oak Ridge Associated Universities through a contract with NASA.; This
work was supported in part by Russian Foundation of Fundamental
Research, grant RFBR 14-02-31546, 14-02-91172.; The KW experiment is
partially supported by a Russian Space Agency contract, RFBR grants
15-02-00532a and 13-02-12017 ofi-m.; Part of the funding for GROND (both
hardware and personnel) was generously granted from the Leibniz-Prize to
Professor G. Hasinger (DFG grant HA 1850/28-1).; AJC acknowledges
support from the Spanish Ministry Grant AYA 2012-39727-C03-01.; CD
acknowledges support through EXTraS, funded from the European Union's
Seventh Framework Programme for research, technological development and
demonstration under grant agreement no 607452.; DAK, SK, and SS
acknowledge support by DFG grants Kl 766/16-1 and 766/16-3. In addition,
SS acknowledges support by the Thuringer Ministerium fur Bildung,
Wissenschaft und Kultur under FKZ 12010-514.; We acknowledge A.
Burenkov, V. Vlasyuk and T. Fatkhullin for the help in observations. AM,
VK and TS are partially supported by the Research Program OFN-17 of the
Division of Physics, Russian Academy of Sciences. AM is also partially
supported by the grant MK-1699.2014.2 of the President of Russian
Federation and by RFBR 14-32-50547.; SS 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 57
TC 4
Z9 4
U1 4
U2 11
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 1
PY 2016
VL 455
IS 1
BP 712
EP 724
DI 10.1093/mnras/stv2228
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900082
ER
PT J
AU Werner, N
ZuHone, JA
Zhuravleva, I
Ichinohe, Y
Simionescu, A
Allen, SW
Markevitch, M
Fabian, AC
Keshet, U
Roediger, E
Ruszkowski, M
Sanders, JS
AF Werner, N.
ZuHone, J. A.
Zhuravleva, I.
Ichinohe, Y.
Simionescu, A.
Allen, S. W.
Markevitch, M.
Fabian, A. C.
Keshet, U.
Roediger, E.
Ruszkowski, M.
Sanders, J. S.
TI Deep Chandra observation and numerical studies of the nearest cluster
cold front in the sky
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; instabilities; galaxies: clusters: individual: Virgo;
galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
ID KELVIN-HELMHOLTZ INSTABILITIES; X-RAY SPECTROSCOPY; GALAXY CLUSTERS;
MAGNETIC-FIELD; THERMAL CONDUCTION; INTERGALACTIC MEDIUM; PERSEUS
CLUSTER; VIRGO CLUSTER; XMM-NEWTON; GAS
AB We present the results of a very deep (500 ks) Chandra observation, along with tailored numerical simulations, of the nearest, best resolved cluster cold front in the sky, which lies 90 kpc (19 arcmin) to the north-west of M87. The northern part of the front appears the sharpest, with a width smaller than 2.5 kpc (1.5 Coulomb mean free paths; at 99 per cent confidence). Everywhere along the front, the temperature discontinuity is narrower than 4-8 kpc and the metallicity gradient is narrower than 6 kpc, indicating that diffusion, conduction and mixing are suppressed across the interface. Such transport processes can be naturally suppressed by magnetic fields aligned with the cold front. Interestingly, comparison to magnetohydrodynamic simulations indicates that in order to maintain the observed sharp density and temperature discontinuities, conduction must also be suppressed along the magnetic field lines. However, the northwestern part of the cold front is observed to have a non-zero width. While other explanations are possible, the broadening is consistent with the presence of Kelvin-Helmholtz instabilities (KHI) on length-scales of a few kpc. Based on comparison with simulations, the presence of KHI would imply that the effective viscosity of the intracluster medium is suppressed by more than an order of magnitude with respect to the isotropic Spitzer-like temperature dependent viscosity. Underneath the cold front, we observe quasi-linear features that are similar to 10 per cent brighter than the surrounding gas and are separated by similar to 15 kpc from each other in projection. Comparison to tailored numerical simulations suggests that the observed phenomena may be due to the amplification of magnetic fields by gas sloshing in wide layers below the cold front, where the magnetic pressure reaches similar to 5-10 per cent of the thermal pressure, reducing the gas density between the bright features.
C1 [Werner, N.; Zhuravleva, I.; Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Werner, N.; Zhuravleva, I.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[ZuHone, J. A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Ichinohe, Y.; Simionescu, A.] JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ichinohe, Y.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Markevitch, M.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Keshet, U.] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel.
[Roediger, E.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Roediger, E.] Dublin Inst Adv Studies, Astron & Astrophys Sect, Dublin 2, Ireland.
[Ruszkowski, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Ruszkowski, M.] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA.
[Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Werner, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA.
EM norbertw@stanford.edu
OI Sanders, Jeremy/0000-0003-2189-4501
FU National Aeronautics and Space Administration [GO3-14142A]; National
Aeronautics Space Administration [NAS8-03060]; NASA [SV2-8203]; ISM of
the DFG (German Research Foundation); Smithsonian Astrophysical
Observatory; European Union; IAEC-UPBC; ISF-UGC; US Department of Energy
[DE-AC02-76SF00515]
FX NW thanks G. Ogrean, P. Nulsen, O. Urban, and R. Canning for
discussions. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO3-14142A 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. JAZ acknowledges support from NASA though subcontract
SV2-8203 to MIT from the Smithsonian Astrophysical Observatory. Analysis
of the simulation data was carried out using YT, a visualization and
analysis software suite for simulations in astrophysics
(http://yt-project.org; Turk et al. 2011). YI is financially supported
by a Grant-in-Aid for Japan Society for the Promotion of Science (JSPS)
Fellows. ER acknowledges the support of the Priority Programme Physics
of the ISM of the DFG (German Research Foundation) and a visiting
scientist fellowship of the Smithsonian Astrophysical Observatory. UK is
supported by the European Union Seventh Framework Programme, by an
IAEC-UPBC joint research foundation grant, and by an ISF-UGC grant. This
work was supported in part by the US Department of Energy under contract
number DE-AC02-76SF00515.
NR 51
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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 JAN 1
PY 2016
VL 455
IS 1
BP 846
EP 858
DI 10.1093/mnras/stv2358
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900091
ER
PT J
AU De Pasquale, M
Oates, SR
Racusin, JL
Kann, DA
Zhang, B
Pozanenko, A
Volnova, AA
Trotter, A
Frank, N
Cucchiara, A
Troja, E
Sbarufatti, B
Butler, NR
Schulze, S
Cano, Z
Page, MJ
Castro-Tirado, AJ
Gorosabel, J
Lien, A
Fox, O
Littlejohns, O
Bloom, JS
Prochaska, JX
de Diego, JA
Gonzalez, J
Richer, MG
Roman-Zuniga, C
Watson, AM
Gehrels, N
Moseley, H
Kutyrev, A
Zane, S
Hoette, V
Russell, RR
Rumyantsev, V
Klunko, E
Burkhonov, O
Breeveld, AA
Reichart, DE
Haislip, JB
AF De Pasquale, M.
Oates, S. R.
Racusin, J. L.
Kann, D. A.
Zhang, B.
Pozanenko, A.
Volnova, A. A.
Trotter, A.
Frank, N.
Cucchiara, A.
Troja, E.
Sbarufatti, B.
Butler, N. R.
Schulze, S.
Cano, Z.
Page, M. J.
Castro-Tirado, A. J.
Gorosabel, J.
Lien, A.
Fox, O.
Littlejohns, O.
Bloom, J. S.
Prochaska, J. X.
de Diego, J. A.
Gonzalez, J.
Richer, M. G.
Roman-Zuniga, C.
Watson, A. M.
Gehrels, N.
Moseley, H.
Kutyrev, A.
Zane, S.
Hoette, V.
Russell, R. R.
Rumyantsev, V.
Klunko, E.
Burkhonov, O.
Breeveld, A. A.
Reichart, D. E.
Haislip, J. B.
TI The central engine of GRB 130831A and the energy breakdown of a
relativistic explosion
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; shock waves; gamma-ray burst:
general; gamma-ray burst: individual: GRB 130831A; stars: magnetars
ID GAMMA-RAY BURST; MAGNETAR CENTRAL ENGINE; SWIFT XRT DATA;
CONFIDENCE-LIMITS; PROTO-MAGNETARS; LIGHT CURVES; DATA RELEASE;
BLACK-HOLES; AFTERGLOW; TELESCOPE
AB Gamma-ray bursts (GRBs) are the most luminous explosions in the Universe, yet the nature and physical properties of their energy sources are far from understood. Very important clues, however, can be inferred by studying the afterglows of these events. We present optical and X-ray observations of GRB 130831A obtained by Swift, Chandra, Skynet, Reionization And Transients Infra-Red camera, Maidanak, International Scientific Optical-Observation Network, Nordic Optical Telescope, Liverpool Telescope and Gran Telescopio Canarias. This burst shows a steep drop in the X-ray light curve at similar to 10(5) s after the trigger, with a power-law decay index of a similar to 6. Such a rare behaviour cannot be explained by the standard forward shock (FS) model and indicates that the emission, up to the fast decay at 105 s, must be of 'internal origin', produced by a dissipation process within an ultrarelativistic outflow. We propose that the source of such an outflow, which must produce the X-ray flux for similar to 1 d in the cosmological rest frame, is a newly born magnetar or black hole. After the drop, the faint X-ray afterglow continues with a much shallower decay. The optical emission, on the other hand, shows no break across the X-ray steep decrease, and the late-time decays of both the X-ray and optical are consistent. Using both the X-ray and optical data, we show that the emission after similar to 10(5) s can be explained well by the FS model. We model our data to derive the kinetic energy of the ejecta and thus measure the efficiency of the central engine of a GRB with emission of internal origin visible for a long time. Furthermore, we break down the energy budget of this GRB into the prompt emission, the late internal dissipation, the kinetic energy of the relativistic ejecta, and compare it with the energy of the associated supernova, SN 2013 fu.
C1 [De Pasquale, M.; Oates, S. R.; Page, M. J.; Zane, S.; Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[De Pasquale, M.] Ist Astrofis Spaziale Fis Cosm, I-90146 Palermo, Italy.
[De Pasquale, M.] Ist Euro Mediterraneo Sci & Tecnol, I-90139 Palermo, Italy.
[Oates, S. R.] CSIC, Ist Astrofis Andalucia, E-18008 Granada, Spain.
[Racusin, J. L.; Cucchiara, A.; Troja, E.; Lien, A.; Gehrels, N.; Moseley, H.; Kutyrev, A.] CRESST, Greenbelt, MD 20771 USA.
[Cucchiara, A.; Troja, E.; Lien, A.; Gehrels, N.; Moseley, H.; Kutyrev, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Pozanenko, A.; Volnova, A. A.] Space Res Inst IKI, Moscow 117997, Russia.
[Pozanenko, A.] Natl Res Nucl Univ MEPhI, Moscow Engn Phys Inst, Moscow 115409, Russia.
[Trotter, A.; Frank, N.; Reichart, D. E.; Haislip, J. B.] Univ N Carolina, Chapel Hill, NC 27599 USA.
[Sbarufatti, B.] Penn State Univ, University Pk, PA 16802 USA.
[Butler, N. R.; Littlejohns, O.] Arizona State Univ, Tempe, AZ 85281 USA.
[Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile.
[Schulze, S.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[Castro-Tirado, A. J.] Univ Malaga, Unidad Asociada, Dept Ingn Sistemas & Automat, E-29071 Malaga, Spain.
[Gorosabel, J.] Univ Basque Country, Unidad Asociada, Grp Ciencia Planetarias, Dept Fis Aplicada 1,ETS Ingn,UPV EHU IAA CSIC, E-48013 Bilbao, Spain.
[Gorosabel, J.] Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain.
[Lien, A.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Fox, O.; Bloom, J. S.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Prochaska, J. X.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[de Diego, J. A.; Gonzalez, J.; Watson, A. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Roman-Zuniga, C.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Hoette, V.; Russell, R. R.] Univ Chicago, Chicago, IL 60637 USA.
[Rumyantsev, V.] Crimean Astrophys Observ, UA-98409 Pgt Nauchny, Crimea, Ukraine.
[Klunko, E.] Russian Acad Sci, Inst Solar Terr Phys, Irkutsk 664033, Russia.
[Burkhonov, O.] Ulugh Beg Astron Inst, Tashkent, Uzbekistan.
RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
EM m.depasquale@ucl.ac.uk; zewcano@gmail.com
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; Rumyantsev, Vasilij/0000-0003-1894-7019;
Schulze, Steve/0000-0001-6797-1889; Sbarufatti,
Boris/0000-0001-6620-8347
FU RFBR [12-0201336, 13-01-92204, 14-02-10015, 15-02-10203]; UK Space
Agency; Spanish Ministry [AYA 2012-39727-C03-01]; CONICYT-Chile FONDECYT
[3140534]; Basal-CATA [PFB-06/2007]; Iniciativa Cientifica Milenio del
Ministerio de Economia, Fomento y Turismo [IC120009]; Thuringer
Landessternwarte Tautenburg; Max-Planck Institut fur Extraterrestrische
Physik; Icelandic Research Fund; NASA [NNX09AH71G, NNX09AT02G,
NNX10AI27G, NNX12AE66G]; CONACyT [NFR-2009-01-122785, CB-2008-101958];
UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT [CN 09-283]; Robert Martin
Ayers Sciences Fund
FX We thank H. Tananbaum for granting us DDT observations of GRB 130831A
with Chandra. This research has made use of data obtained from the
Chandra Data Archive and the Chandra Source Catalog, and software
provided by the Chandra X-ray Center (CXC) in the application packages
CIAO, CHIPS, and SHERPA.; MDP, MJP, SRO and AAB thank UK Space Agency
for financial support. This work made use of data supplied by the UK
Swift Science Data Centre at the University of Leicester.; AP, AV
acknowledge partial support by RFBR grants 12-0201336, 13-01-92204,
14-02-10015 and 15-02-10203.; AJCT and SRO acknowledges support from the
Spanish Ministry Grant AYA 2012-39727-C03-01.; SS 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.; DAK
acknowledges financial support by the Thuringer Landessternwarte
Tautenburg, and the Max-Planck Institut fur Extraterrestrische Physik.;
ZC gratefully acknowledges support by a Project Grant from the Icelandic
Research Fund.; We thank the RATIR project team and the staff of the
Observatorio Astronmico Nacional on Sierra San Pedro Martir. RATIR is a
collaboration between the University of California, the Universidad
Nacional Autonoma de Mexico, NASA Goddard Space Flight Center, and
Arizona State University, benefiting from the loan of an H2RG detector
and hardware and software support from Teledyne Scientific and Imaging.
RATIR, the automation of the Harold L. Johnson Telescope of the
Observatorio Astronmico Nacional on Sierra San Pedro Martir, and the
operation of both are funded through NASA grants NNX09AH71G, NNX09AT02G,
NNX10AI27G, and NNX12AE66G, CONACyT grants INFR-2009-01-122785 and
CB-2008-101958, UNAM PAPIIT grant IN113810, and UC MEXUS-CONACyT grant
CN 09-283.; Partly based on observations carried out with the 10.4 m GTC
installed in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias in the island of La Palma. Partly
based on the AAVSO Photometric All-Sky Survey (APASS), funded by the
Robert Martin Ayers Sciences Fund.
NR 105
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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 1
PY 2016
VL 455
IS 1
BP 1027
EP 1042
DI 10.1093/mnras/stv2280
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900103
ER
PT J
AU Pope, BJS
White, TR
Huber, D
Murphy, SJ
Bedding, TR
Caldwell, DA
Sarai, A
Aigrain, S
Barclay, T
AF Pope, B. J. S.
White, T. R.
Huber, D.
Murphy, S. J.
Bedding, T. R.
Caldwell, D. A.
Sarai, A.
Aigrain, S.
Barclay, T.
TI Photometry of very bright stars with Kepler and K2 smear data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE asteroseismology; techniques: photometric; stars: individual: HR 8500,
70 Aqr, HD 178875; stars: variables: general
ID EFFECTIVE TEMPERATURE SCALE; SOLAR-LIKE OSCILLATIONS; RED-GIANT STARS;
GALACTIC ARCHAEOLOGY; STELLAR POPULATIONS; CHARA ARRAY; MISSION;
ASTEROSEISMOLOGY; PERFORMANCE; AMPLITUDES
AB High-precision time series photometry with the Kepler satellite has been crucial to our understanding both of exoplanets, and via asteroseismology, of stellar physics. After the failure of two reaction wheels, the Kepler satellite has been repurposed as Kepler-2 (K2), observing fields close to the ecliptic plane. As these fields contain many more bright stars than the original Kepler field, K2 provides an unprecedented opportunity to study nearby objects amenable to detailed follow-up with ground-based instruments. Due to bandwidth constraints, only a small fraction of pixels can be downloaded, with the result that most bright stars which saturate the detector are not observed. We show that engineering data acquired for photometric calibration, consisting of collateral `smear' measurements, can be used to reconstruct light curves for bright targets not otherwise observable with Kepler/K2. Here we present some examples from Kepler Quarter 6 and K2 Campaign 3, including the delta Scuti variables HD 178875 and 70 Aqr, and the red giant HR 8500 displaying solar-like oscillations. We compare aperture and smear photometry where possible, and also study targets not previously observed. These encouraging results suggest this new method can be applied to most Kepler and K2 fields.
C1 [Pope, B. J. S.; Aigrain, S.] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England.
[White, T. R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[White, T. R.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Huber, D.; Murphy, S. J.; Bedding, T. R.; Sarai, A.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Huber, D.; Caldwell, D. A.] SETI Inst, Mountain View, CA 94043 USA.
[Huber, D.; Murphy, S. J.; Bedding, T. R.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Caldwell, D. A.; Barclay, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, T.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
RP Pope, BJS (reprint author), Univ Oxford, Oxford Astrophys, Keble Rd, Oxford OX1 3RH, England.
EM benjamin.pope@astro.ox.ac.uk
OI Murphy, Simon/0000-0002-5648-3107; Pope, Benjamin/0000-0003-2595-9114;
Sarai, Aleksa/0000-0003-4811-6339
FU NASA [NAS5-26555, NNX14AB92G]; NASA Office of Space Science
[NNX13AC07G]; German Academic Exchange Service through the Go8
Australia-Germany Joint Research Co-operation Scheme; Australian
Research Council [DE140101364]
FX This research made use of NASA's Astrophysics Data System; the SIMBAD
data base, operated at CDS, Strasbourg, France; the IPYTHON package
(Perez & Granger 2007); SciPy (Jones et al. 2001). 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 NNX13AC07G and by
other grants and contracts. We acknowledge the support of the Group of
Eight universities and the German Academic Exchange Service through the
Go8 Australia-Germany Joint Research Co-operation Scheme. DH
acknowledges support by the Australian Research Council's Discovery
Projects funding scheme (project number DE140101364) and support by the
NASA Grant NNX14AB92G issued through the Kepler Participating Scientist
Program.
NR 44
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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 1
PY 2016
VL 455
IS 1
BP L36
EP L40
DI 10.1093/mnrasl/slv143
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7TB
UT WOS:000368005900008
ER
PT J
AU Yoon, J
Pozzer, A
Chang, DY
Lelieveld, J
Kim, J
Kim, M
Lee, YG
Koo, JH
Lee, J
Moon, KJ
AF Yoon, J.
Pozzer, A.
Chang, D. Y.
Lelieveld, J.
Kim, J.
Kim, M.
Lee, Y. G.
Koo, J. -H.
Lee, J.
Moon, K. J.
TI Trend estimates of AERONET-observed and model-simulated AOTs between
1993 and 2013
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol optical thickness; AErosol RObotic NETwork; ECHAM/MESSy
atmospheric chemistry model; Trend estimates; Monthly percentiles;
Monthly cumulative distributions
ID AEROSOL OPTICAL DEPTH; CHEMISTRY-CLIMATE MODEL; GLOBAL FIRE EMISSIONS;
DESERT DUST; RAIN-FOREST; WET SEASON; SURFACE; AREA; VARIABILITY;
ABSORPTION
AB Recently, temporal changes in Aerosol Optical Thickness (AOT) have been investigated based on model simulations, satellite and ground-based observations. Most AOT trend studies used monthly or annual arithmetic means that discard details of the generally right-skewed AOT distributions. Potentially, such results can be biased by extreme values (including outliers). This study additionally uses percentiles (i.e., the lowest 5%, 25%, 50%, 75% and 95% of the monthly cumulative distributions fitted to Aerosol Robotic Network (AERONET)-observed and ECHAM/MESSy Atmospheric Chemistry (EMAC)-model simulated AOTs) that are less affected by outliers caused by measurement error, cloud contamination and occasional extreme aerosol events. Since the limited statistical representativeness of monthly percentiles and means can lead to bias, this study adopts the number of observations as a weighting factor, which improves the statistical robustness of trend estimates. By analyzing the aerosol composition of AERONET-observed and EMAC-simulated AOTs in selected regions of interest, we distinguish the dominant aerosol types and investigate the causes of regional AOT trends. The simulated and observed trends are generally consistent with a high correlation coefficient (R = 0.89) and small bias (slope +/- 2 sigma = 0.75 +/- 0.19). A significant decrease in EMAC-decomposed AOTs by water-soluble compounds and black carbon is found over the USA and the EU due to environmental regulation. In particular, a clear reversal in the AERONET AOT trend percentiles is found over the USA, probably related to the AOT diurnal cycle and the frequency of wildfires. In most of the selected regions of interest, EMAC-simulated trends are mainly attributed to the significant changes of the dominant aerosols; e.g., significant decrease in sea salt and water soluble compounds over Central America, increase in dust over Northern Africa and Middle East, and decrease in black carbon and organic carbon over Australia. (C) 2015 The Authors. Published by Elsevier Ltd.
C1 [Yoon, J.; Pozzer, A.; Chang, D. Y.; Lelieveld, J.] Max Planck Inst Chem, Atmospher Chem Dept, D-55020 Mainz, Germany.
[Lelieveld, J.] Cyprus Inst, CY-1645 Nicosia, Cyprus.
[Lelieveld, J.] King Saud Univ, Riyadh 11451, Saudi Arabia.
[Kim, J.; Kim, M.] Yonsei Univ, Dept Atmosphere Sci IEAA BK Plus 21, Seoul 120749, South Korea.
[Lee, Y. G.] Chungnam Natl Univ, Res Inst Basic Sci, Daejeon, South Korea.
[Koo, J. -H.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Lee, J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Lee, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moon, K. J.] NIER, Inchon, South Korea.
RP Yoon, J (reprint author), Max Planck Inst Chem, Atmospher Chem Dept, POB 3060, D-55020 Mainz, Germany.
EM jongmin.yoon@mpic.de
RI Pozzer, Andrea/L-4872-2013; Lelieveld, Johannes/A-1986-2013;
OI Pozzer, Andrea/0000-0003-2440-6104; Lee, Jaehwa/0000-0002-5029-476X
FU Korea Meteorological Administration Research and Development Program
Grant KMIPA [KMIPA2015-5010]
FX The authors would like to thank the AERONET for its effort in
establishing and maintaining all sites selected in this study. We
gratefully acknowledge the efforts of the EMAC development team to
develop and make available the EMAC modeling system. We also thank the
MPIC Satellite group for comments that helped improve the manuscript.
This work was funded by the Korea Meteorological Administration Research
and Development Program under Grant KMIPA KMIPA2015-5010. The article
processing charges for this publication were covered by the Max Planck
Society.
NR 105
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD JAN
PY 2016
VL 125
BP 33
EP 47
DI 10.1016/j.atmosenv.2015.10.058
PN A
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DA2OU
UT WOS:000367636500005
ER
PT J
AU Tao, ZN
Yu, HB
Chin, M
AF Tao, Zhining
Yu, Hongbin
Chin, Mian
TI Impact of transpacific aerosol on air quality over the United States: A
perspective from aerosol-cloud-radiation interactions
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Transpacific aerosol; Aerosol-cloud-radiation interactions; NU-WRF; US
air quality
ID INTERCONTINENTAL TRANSPORT; NORTH-AMERICA; DUST AEROSOLS; GLOBAL-MODELS;
GOCART MODEL; EAST-ASIA; WRF MODEL; NU-WRF; POLLUTION; EMISSIONS
AB Observations have well established that aerosols from various sources in Asia, Europe, and Africa can travel across the Pacific and reach the contiguous United States (U.S.) at least on episodic bases throughout a year, with a maximum import in spring. The imported aerosol not only can serve as an additional source to regional air pollution (e.g., direct input), but also can influence regional air quality through the aerosol-cloud-radiation (ACR) interactions that change local and regional meteorology. This study assessed impacts of the transpacific aerosol on air quality, focusing on surface ozone and PM2.5, over the U.S. using the NASA Unified Weather Research Forecast model. Based on the results of 3-month (April to June of 2010) simulations, the impact of direct input (as an additional source) of transpacific aerosol caused an increase of surface PM2.5 concentration by approximately 1.5 mu g m(-3) over the west coast and about 0.5 mu g m(-3) over the east coast of the U.S. By influencing key meteorological processes through the ACR interactions, the transpacific aerosol exerted a significant effect on both surface PM2.5 (+/- 6 mu g m(-3)) and ozone (+/- 12 ppbv) over the central and eastern U.S. This suggests that the transpacific transport of aerosol could either improve or deteriorate local air quality and complicate local effort toward the compliance with the U.S. National Ambient Air Quality Standards. (c) 2015 Elsevier Ltd. All rights reserved.
C1 [Tao, Zhining] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Tao, Zhining; Yu, Hongbin; Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
RP Tao, ZN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM zhining.tao@nasa.gov
RI Yu, Hongbin/C-6485-2008; Chin, Mian/J-8354-2012
OI Yu, Hongbin/0000-0003-4706-1575;
FU NASA's Atmospheric Composition: Modeling and Analysis (ACMAP) program;
Modeling, Analysis, and Prediction (MAP) program
FX The authors would like to thank the NASA Center for Climate Simulation
(NCCS) for supercomputing support. This research was funded by NASA's
Atmospheric Composition: Modeling and Analysis (ACMAP) program and the
Modeling, Analysis, and Prediction (MAP) program. Helpful discussions
with Drs. Jainn Shi and Toshihisa Matsui of GSFC were also greatly
appreciated.
NR 49
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U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD JAN
PY 2016
VL 125
BP 48
EP 60
DI 10.1016/j.atmosenv.2015.10.083
PN A
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DA2OU
UT WOS:000367636500006
ER
PT J
AU Buchard, V
da Silva, AM
Randles, CA
Colarco, P
Ferrare, R
Hair, J
Hostetler, C
Tackett, J
Winker, D
AF Buchard, V.
da Silva, A. M.
Randles, C. A.
Colarco, P.
Ferrare, R.
Hair, J.
Hostetler, C.
Tackett, J.
Winker, D.
TI Evaluation of the surface PM2.5 in Version 1 of the NASA MERRA Aerosol
Reanalysis over the United States
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air pollution; Aerosols; Particulate mater; MERRAero; MODIS; AERONET
ID DATA ASSIMILATION SYSTEM; FINE PARTICULATE MATTER; OPTICAL DEPTH;
SATELLITE-OBSERVATIONS; AIR-POLLUTION; QUALITY; MODELS; IMPACT;
THICKNESS; LIDAR
AB We use surface fine particulate matter (PM2.5) measurements collected by the United States Environmental Protection Agency (US EPA) and the Interagency Monitoring of Protected Visual Environments (IMPROVE) networks as independent validation for Version 1 of the Modern Era Retrospective analysis for Research and Applications Aerosol Reanalysis (MERRAero) developed by the Global Modeling Assimilation Office (GMAO). MERRAero is based on a version of the GEOS-5 model that is radiatively coupled to the Goddard Chemistry, Aerosol, Radiation, and Transport (GOCART) aerosol module and includes assimilation of bias corrected Aerosol Optical Depth (AOD) from Moderate Resolution Imaging Spectroradiometer (MODIS) sensors on both Terra and Aqua satellites. By combining the spatial and temporal coverage of GEOS-5 with observational constraints on AOD, MERRAero has the potential to provide improved estimates of PM2.5 compared to the model alone and with greater coverage than available observations.
Importantly, assimilation of AOD data constrains the total column aerosol mass in MERRAero subject to assumptions about optical properties for each of the species represented in GOGART. However, single visible wavelength AOD data does not contain sufficient information content to correct errors in either aerosol vertical placement or composition, critical elements for a proper characterization of surface PM2.5 Despite this, we find that the data-assimilation equipped version of GEOS-5 better represents observed PM2.5 between 2003 and 2012 compared to the same version of the model without AOD assimilation. Compared to measurements from the EPA-AQS network, MERRAero shows better PM2.5 agreement with the IMPROVE network measurements, which are composed essentially of rural stations. Regardless the data network, MERRAero PM2.5 are closer to observation values during the summer while larger discrepancies are observed during the winter. Comparing MERRAero to PM2.5 data collected by the Chemical Speciation. Network (CSN) offers greater insight on the species MERRAero predicts well and those for which there are biases relative to the EPA observations. Analysis of this speciated data indicates that the lack of nitrate emissions in MERRAero and an underestimation of carbonaceous emissions in the Western US explains much of the reanalysis bias during the winter. To further understand discrepancies between the reanalysis and observations, we use complimentary data to assess two important aspects of MERRAero that are of relevance to the diagnosis of PM2.5, in particular AOD and vertical structure. (c) 2015 Elsevier Ltd. All rights reserved.
C1 [Buchard, V.; da Silva, A. M.; Randles, C. A.; Colarco, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Buchard, V.] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Randles, C. A.] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
[Ferrare, R.; Hair, J.; Hostetler, C.; Tackett, J.; Winker, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Tackett, J.] SSAI, Hampton, VA USA.
RP Buchard, V (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM virginie.buchard@nasa.gov
RI Colarco, Peter/D-8637-2012
OI Colarco, Peter/0000-0003-3525-1662
NR 48
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U1 7
U2 32
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD JAN
PY 2016
VL 125
BP 100
EP 111
DI 10.1016/j.atmosenv.2015.11.004
PN A
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DA2OU
UT WOS:000367636500011
ER
PT J
AU Zwart, SR
Gregory, JF
Zeisel, SH
Gibson, CR
Mader, TH
Kinchen, JM
Ueland, PM
Ploutz-Snyder, R
Heer, MA
Smith, SM
AF Zwart, Sara R.
Gregory, Jesse F.
Zeisel, Steven H.
Gibson, Charles R.
Mader, Thomas H.
Kinchen, Jason M.
Ueland, Per M.
Ploutz-Snyder, Robert
Heer, Martina A.
Smith, Scott M.
TI Genotype, B-vitamin status, and androgens affect spaceflight-induced
ophthalmic changes
SO FASEB JOURNAL
LA English
DT Article
ID POLYCYSTIC-OVARY-SYNDROME; IDIOPATHIC INTRACRANIAL HYPERTENSION;
DURATION SPACE-FLIGHT; SECONDARY PSEUDOTUMOR CEREBRI; SEXUAL
REASSIGNMENT THERAPY; ONE-CARBON METABOLISM; METHYLENETETRAHYDROFOLATE
REDUCTASE; BED REST; HOMOCYSTEINE; WOMEN
AB Ophthalmic changes have occurred in a subset of astronauts on International Space Station missions. Visual deterioration is considered the greatest human health risk of spaceflight. Affected astronauts exhibit higher concentrations of 1-carbon metabolites (e.g., homocysteine) before flight. We hypothesized that genetic variations in 1-carbon metabolism genes contribute to susceptibility to ophthalmic changes in astronauts. We investigated 5 polymorphisms in the methionine synthase reductase (MTRR), methylenetetrahydrofolate reductase (MTHFR), serine hydroxymethyltransferase (SHMT), and cystathionine beta-synthase (CBS) genes and their association with ophthalmic changes after flight in 49 astronauts. The number of G alleles of MTRR 66 and C alleles of SHMT1 1420 both contributed to the odds of visual disturbances. Preflight dehydroepiandrosterone was positively associated with cotton wool spots, and serum testosterone response during flight was associated with refractive change. Block regression showed that B-vitamin status and genetics were significant predictors of many of the ophthalmic outcomes that we observed. In one example, genetics trended toward improving (P = 0.10) and B-vitamin status significantly improved (P < 0.001) the predictive model for refractive change after flight. We document an association between MTRR 66 and SHMT1 1420 polymorphisms and spaceflight-induced vision changes. This line of research could lead to therapeutic options for both space travelers and terrestrial patients.-Zwart, S. R., Gregory, J. F., Zeisel, S. H., Gibson, C. R., Mader, T. H., Kinchen, J. M., Ueland, P. M., Ploutz-Snyder, R., Heer, M. A., Smith, S. M. Genotype, B-vitamin status, and androgens affect spaceflight-induced ophthalmic changes. FASEB J. 30, 141-148 (2016). www.fasebj.org
C1 [Zwart, Sara R.; Ploutz-Snyder, Robert] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Gregory, Jesse F.] Univ Florida, Inst Food & Agr Sci, Food Sci & Human Nutr, Gainesville, FL 32611 USA.
[Zeisel, Steven H.] Univ N Carolina, Inst Nutr Res, Kannapolis, NC USA.
[Gibson, Charles R.] Coastal Eye Associates, Webster, TX USA.
[Kinchen, Jason M.] Metabolon Inc, Durham, NC USA.
[Ueland, Per M.] Univ Bergen, Dept Clin Sci, Bergen, Norway.
[Heer, Martina A.] Univ Bonn, Dept Nutr & Food Sci, Nutrit Physiol, Bonn, Germany.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
RI Ueland, Per/C-7340-2013
FU NASA Human Research Program's Human Health and Countermeasures Element;
German Federal Ministry for Economics and Technology/DLR Forschung unter
Weltraumbedingungen [50WB0931]; U.S. National Institutes of Health,
National Institute of Diabetes and Digestive and Kidney Diseases
[DK56350]
FX The authors thank the astronauts for their participation in and support
of this study; the staff of the NASA Johnson Space Center Nutritional
Biochemistry Laboratory for their assistance in all aspects of the
project; the ISS Medical Project, specifically T. Bauer, for help with
coordinating the project; the NASA Lifetime Surveillance of Astronaut
Health team for their help with eye- and vision-related data; and J.
Krauhs for editorial assistance. This project was funded by the NASA
Human Research Program's Human Health and Countermeasures Element, by
the German Federal Ministry for Economics and Technology/DLR Forschung
unter Weltraumbedingungen Grant 50WB0931 (to M.A.H.), and by the U.S.
National Institutes of Health, National Institute of Diabetes and
Digestive and Kidney Diseases Grant DK56350 (to S.H.Z.). S.M.S., S.R.Z.,
and M.A.H. designed the research; S.M.S. and S.R.Z. oversaw data
collection and management of the biological sample collections and
analyses; C.R.G. and T.H.M. oversaw data collection and management of
the vision and related data; J.M.K. conducted metabolomics analyses; and
R.P.S. performed statistical analysis; and all authors were involved in
interpreting the data and preparing the manuscript. All authors read and
approved the final manuscript. S.M.S. had primary responsibility for the
content of the final version. The authors declare no conflicts of
interest.
NR 38
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PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
EI 1530-6860
J9 FASEB J
JI Faseb J.
PD JAN
PY 2016
VL 30
IS 1
BP 141
EP 148
DI 10.1096/fj.15-278457
PG 8
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA DA2JL
UT WOS:000367621000016
PM 26316272
ER
PT J
AU Elsila, JE
Callahan, MP
Dworkin, JP
Glavin, DP
McLain, HL
Noble, SK
Gibson, EK
AF Elsila, Jamie E.
Callahan, Michael P.
Dworkin, Jason P.
Glavin, Daniel P.
McLain, Hannah L.
Noble, Sarah K.
Gibson, Everett K., Jr.
TI The origin of amino acids in lunar regolith samples
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID SOLAR-SYSTEM; CARBONACEOUS CHONDRITES; ISOTOPIC COMPOSITION; MURCHISON
METEORITE; EXOGENOUS DELIVERY; MASS SPECTROMETRY; ORGANIC-MOLECULES;
IMPACT DELIVERY; EXTRATERRESTRIAL; CONTAMINATION
AB We analyzed the amino acid content of seven lunar regolith samples returned by the Apollo 16 and Apollo 17 missions and stored under NASA curation since collection using ultrahigh-performance liquid chromatography with fluorescence detection and time-of-flight mass spectrometry. Consistent with results from initial analyses shortly after collection in the 1970s, we observed amino acids at low concentrations in all of the curated samples, ranging from 0.2 parts-per-billion (ppb) to 42.7 ppb in hot-water extracts and 14.5-651.1 ppb in 6 M HCl acid-vapor-hydrolyzed, hot-water extracts. Amino acids identified in the Apollo soil extracts include glycine, D-and L-alanine, D-and L-aspartic acid, D-and L-glutamic acid, D-and L-serine, L-threonine, and L-valine, all of which had previously been detected in lunar samples, as well as several compounds not previously identified in lunar regoliths: alpha-aminoisobutyric acid (AIB), D-and L-b-amino-n-butyric acid (beta-ABA), DL-alpha-amino-n-butyric acid, gamma-amino-n-butyric acid, beta-alanine, and epsilon-amino-n-caproic acid. We observed an excess of the L enantiomer in most of the detected proteinogenic amino acids, but racemic alanine and racemic beta-ABA were present in some samples.
We also examined seven samples from Apollo 15, 16, and 17 that had been previously allocated to a non-curation laboratory, as well as two samples of terrestrial dunite from studies of lunar module engine exhaust that had been stored in the same laboratory. The amino acid content of these samples suggested that contamination had occurred during non-curatorial storage.
We measured the compound-specific carbon isotopic ratios of glycine, beta-alanine, and L-alanine in Apollo regolith sample 70011 and found values of -21% to -33%. These values are consistent with those seen in terrestrial biology and, together with the enantiomeric compositions of the proteinogenic amino acids, suggest that terrestrial biological contamination is a primary source of the amino acids in these samples. However, the presence of the non-proteinogenic amino acids such as AIB and b-ABA suggests the possibility of some contribution from exogenous sources.
We did not observe a correlation of amino acid content with proximity to the Apollo 17 lunar module, implying that lunar module exhaust was not a primary source of amino acid precursors. Solar-wind-implanted precursors such as HCN also appear to be at most a minor contributor, given a lack of correlation between amino acid content and soil maturity (as measured by I-s/FeO ratio) and the differences between the delta C-13 values of the amino acids and the solar wind. Published by Elsevier Ltd.
C1 [Elsila, Jamie E.; Callahan, Michael P.; Dworkin, Jason P.; Glavin, Daniel P.; McLain, Hannah L.; Noble, Sarah K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McLain, Hannah L.] Catholic Univ Amer, Washington, DC 20064 USA.
[Gibson, Everett K., Jr.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Elsila, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Jamie.Elsila@nasa.gov
RI Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Dworkin,
Jason/C-9417-2012
OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997
FU NASA's Lunar Advanced Science and Exploration Research (LASER) Program
[11-LASER11-0013]; NASA Astrobiology Institute; Goddard Center for
Astrobiology
FX The authors would like to thank CAPTEM and the NASA Johnson Space Center
lunar sample curator for allocation of the samples analyzed in this
study, and William Farrell for useful discussions. We also thank Randy
Korotev and an anonymous reviewer for thoughtful comments. This research
was supported by NASA's Lunar Advanced Science and Exploration Research
(LASER) Program (11-LASER11-0013), as well as the NASA Astrobiology
Institute and the Goddard Center for Astrobiology.
NR 66
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U1 4
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 1
PY 2016
VL 172
BP 357
EP 369
DI 10.1016/j.gca.2015.10.008
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DA1AP
UT WOS:000367529000020
ER
PT J
AU Norman, MD
Taylor, LA
Shih, CY
Nyquist, LE
AF Norman, M. D.
Taylor, L. A.
Shih, C. -Y.
Nyquist, L. E.
TI Crystal accumulation in a 4.2 Ga lunar impact melt
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; POLE-AITKEN BASIN; NORTH-RAY
CRATER; ION MICROPROBE; TRACE-ELEMENTS; MG-SUITE; PLAGIOCLASE FELDSPAR;
TERRESTRIAL PLANETS; PARENTAL MAGMAS
AB The ages of lunar impact basins and the role of fractional crystallization in producing compositional heterogeneity of lunar melt sheets are long-standing problems with significant implications for solar system dynamics and the petrologic evolution of the lunar crust. Here we document the formation of a basin-scale impact on the Moon at 4.20 +/- 0.07 Ga based on the Sm-147-Nd-143 isochron age of a magnesian, noritic anorthosite melt rock from lunar breccia 67955. Major element compositions of plagioclase and mafic silicates in the melt rock imply a substantial component of primary Mg-suite cumulates or related lithologies in the pre-impact crustal stratigraphy. Trace element compositions of the plagioclase, including diagnostic ratios such as Sr/Ba, are also mostly similar to those in plagioclase from Mg-suite cumulates, with a small number of grains trending toward compositions observed in ferroan anorthosites. Mineral-melt distribution coefficients applied to trace element compositions of the 67955 plagioclase and pyroxene predict parental melt compositions that contrast strongly with the bulk rock. Compared to the whole rock, parental melts calculated from the plagioclase are enriched in REE (Sigma REELa-Yb = 131-885, average 619 ppm vs. 39.8 ppm) and they have more fractionated REE patterns (La/Yb-n = 1.2-9.8, average 4.9 vs. 1.5) with deep negative Eu anomalies (Eu/Eu* = 0.09-0.40 vs. 1.36). Trace element data for the pyroxenes also imply incompatible-element enriched parental melts. Subsolidus equilibration between the plagioclase and the pyroxene apparently rotated the REE patterns, but the conclusion that the parental melt was highly enriched in REE relative to the whole rock appears robust. Quantitative modeling shows that fractional crystallization of the 67955 whole rock composition cannot reproduce the range of Ba, Sr, Ti, and La concentrations measured in the 67955 plagioclase. Rather, the models require an initial melt composition that was strongly enriched in these elements, and they suggest that fractional crystallization became less efficient as crystallization proceeded. The contrast between the inferred parental melt composition and the bulk rock implies formation of the 67955 noritic anorthosite as a crystal cumulate, and that the cogenetic residual melt was strongly enriched in incompatible elements. If so, this would be the first documented example of fractional crystallization in a lunar impact melt sheet. The petrological and geochemical characteristics of the 67955 noritic anorthosite suggest that it formed by an impact in the Procellarum-KREEP Terrane, and was transported to the Apollo 16 site as Imbrium ejecta. Inheritance of ejecta related to this pre-Imbrium basin may contribute to the common occurrence of similar to 4.2 Ga Ar-40-Ar-39 plateau ages in breccia clasts and regolith fragments from the rim of North Ray crater. In that case, those data may provide no constraints on the age of the Nectaris basin, despite its proximity to the Apollo 16 site. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Norman, M. D.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Norman, M. D.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia.
[Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Shih, C. -Y.; Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
RP Norman, MD (reprint author), Australian Natl Univ, Res Sch Earth Sci, GPO Box 4, Canberra, ACT 0200, Australia.
EM Marc.Norman@anu.edu.au
FU NASA Lunar Advanced Science Exploration Research (LASER) Program
[10-LASER10-0054]
FX MN gratefully acknowledges Visiting Scientist support from the Lunar and
Planetary Institute and the Centre for Lunar Science and Exploration at
various times throughout this project. Jessica Bowen-Thomas assisted
with preparation and documentation of polished mounts. Financial support
for L.E.N. and C.-Y.S. was provided by the NASA Lunar Advanced Science
Exploration Research (LASER) Program via proposal number
10-LASER10-0054. We thank James W. Head, William K. Hartmann, Thomas
Haber, and Associate Editor Uwe Reimold for constructive reviews and
comments on the manuscript.
NR 129
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U1 5
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 1
PY 2016
VL 172
BP 410
EP 429
DI 10.1016/j.gca.2015.09.021
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DA1AP
UT WOS:000367529000024
ER
PT J
AU Dickinson, MB
Hudak, AT
Zajkowski, T
Loudermilk, EL
Schroeder, W
Ellison, L
Kremens, RL
Holley, W
Martinez, O
Paxton, A
Bright, BC
O'Brien, JJ
Hornsby, B
Ichoku, C
Faulring, J
Gerace, A
Peterson, D
Mauceri, J
AF Dickinson, Matthew B.
Hudak, Andrew T.
Zajkowski, Thomas
Loudermilk, E. Louise
Schroeder, Wilfrid
Ellison, Luke
Kremens, Robert L.
Holley, William
Martinez, Otto
Paxton, Alexander
Bright, Benjamin C.
O'Brien, Joseph J.
Hornsby, Benjamin
Ichoku, Charles
Faulring, Jason
Gerace, Aaron
Peterson, David
Mauceri, Joseph
TI Measuring radiant emissions from entire prescribed fires with ground,
airborne and satellite sensors - RxCADRE 2012
SO INTERNATIONAL JOURNAL OF WILDLAND FIRE
LA English
DT Article
DE fire behaviour; fire radiative power; MODIS; remote sensing; unmanned
aircraft systems; VIIRS; WASP
ID PIXEL-BASED CALCULATION; RADIATIVE POWER; SENSITIVITY-ANALYSIS; INITIAL
ASSESSMENT; SURFACE FIRES; ACTIVE FIRES; MODIS; ALGORITHM; PRODUCTS;
ENERGY
AB Characterising radiation from wildland fires is an important focus of fire science because radiation relates directly to the combustion process and can be measured across a wide range of spatial extents and resolutions. As part of a more comprehensive set of measurements collected during the 2012 Prescribed Fire Combustion and Atmospheric Dynamics Research (RxCADRE) field campaign, we used ground, airborne and spaceborne sensors to measure fire radiative power (FRP) from whole fires, applying different methods to small (2 ha) and large (>100 ha) burn blocks. For small blocks (n = 6), FRP estimated from an obliquely oriented long-wave infrared (LWIR) camera mounted on a boom lift were compared with FRP derived from combined data from tower-mounted radiometers and remotely piloted aircraft systems (RPAS). For large burn blocks (n = 3), satellite FRP measurements from the Moderate-resolution Imaging Spectroradiometer (MODIS) and Visible Infrared Imaging Radiometer Suite (VIIRS) sensors were compared with near-coincident FRP measurements derived from a LWIR imaging system aboard a piloted aircraft. We describe measurements and consider their strengths and weaknesses. Until quantitative sensors exist for small RPAS, their use in fire research will remain limited. For oblique, airborne and satellite sensors, further FRP measurement development is needed along with greater replication of coincident measurements, which we show to be feasible.
C1 [Dickinson, Matthew B.] USDA Forest Serv, No Res Stn, Delaware, OH 43015 USA.
[Hudak, Andrew T.; Bright, Benjamin C.] USDA Forest Serv, Rocky Mt Res Stn, Forestry Sci Lab, Moscow, ID 83843 USA.
[Zajkowski, Thomas] USDA Forest Serv, Remote Sensing Applicat Ctr, Salt Lake City, UT 84119 USA.
[Loudermilk, E. Louise; O'Brien, Joseph J.; Hornsby, Benjamin] USDA Forest Serv, Ctr Forest Disturbance Sci, Southern Res Ctr, Athens, GA 30602 USA.
[Schroeder, Wilfrid] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Ellison, Luke; Ichoku, Charles] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ellison, Luke] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Kremens, Robert L.; Faulring, Jason; Gerace, Aaron; Mauceri, Joseph] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Holley, William; Martinez, Otto; Paxton, Alexander] US Air Force, Niceville, FL 32542 USA.
[Peterson, David] CNR, Monterey, CA 93943 USA.
RP Dickinson, MB (reprint author), USDA Forest Serv, No Res Stn, 359 Main Rd, Delaware, OH 43015 USA.
EM mbdickinson@fs.fed.us
RI Schroeder, Wilfrid/F-6738-2010; peterson, david/L-2350-2016;
OI Dickinson, Matthew/0000-0003-3635-1219
FU Joint Fire Science Program [11-2-1-11]
FX We thank the Eglin AFB fire management staff, particularly Kevin Hiers,
Brett Williams and the fire crews for their supreme competence in
prescribed burning and logistical coordination. We also thank the many
scientists and support staff not included in this paper whose work and
collaboration made the RxCADRE project possible, particularly Roger
Ottmar who led the effort and Dan Jimenez who facilitated agreements and
funding. It is with sadness and gratitude that we note the loss of Dr
Otto Martinez and Mr. Bill Holley of the Eglin AFB Digital Video
Laboratory. Otto and Bill were central to the planning and
implementation of the complex RxCADRE airborne operations and, in
addition, they coordinated RPAS operations that included multiple
platforms and managed real-time data collection and display. The 2012
RxCADRE campaign was made possible by a grant from the Joint Fire
Science Program (Project #11-2-1-11), and longer-term support from the
US Forest Service, National Fire Plan, Joint Fire Science Program and
NASA was critical for getting the RxCADRE project started. Thanks to
Ellen Eberhardt and several anonymous reviewers for their input on the
manuscript.
NR 52
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U1 6
U2 10
PU CSIRO PUBLISHING
PI CLAYTON
PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC
3168, AUSTRALIA
SN 1049-8001
EI 1448-5516
J9 INT J WILDLAND FIRE
JI Int. J. Wildland Fire
PY 2016
VL 25
IS 1
BP 48
EP 61
DI 10.1071/WF15090
PG 14
WC Forestry
SC Forestry
GA DA3VH
UT WOS:000367727100005
ER
PT J
AU Sentchev, A
Yaremchuk, M
AF Sentchev, Alexei
Yaremchuk, Max
TI Monitoring tidal currents with a towed ADCP system
SO OCEAN DYNAMICS
LA English
DT Article
DE Towed ADCP survey; Tidal currents; English Channel; Optimal
interpolation
ID DOPPLER CURRENT PROFILER; WEST FLORIDA SHELF; SURFACE CURRENTS; ENERGY;
RESOURCE; CHANNEL; FLOW; FIELD; POWER
AB The tidal circulation in the semi-enclosed Boulogne harbour (eastern English Channel) is measured during the various stages of the tidal cycle with a low-cost towed Acoustic Doppler Current Profiler (ADCP) system for the first time. The system is equipped with an interpolation algorithm which allows reconstructing space-time evolution of the velocity field for surveys whose duration is comparable or larger than the typical time of tidal variation (1-2 h). The method employs space-time velocity covariances derived from a numerical simulation of the surveyed area by a high-resolution relocatable model "Model for Applications on Regional Scale" (MARS). The covariances are utilized by the optimal interpolation algorithm to obtain the most likely evolution of the velocity field under the constraints provided by the ADCP observations and their error statistics. Technically, the MARS model run provides the first guess (background) evolution of the velocity field in the surveyed area which is then corrected by the data in a statistically consistent manner as it explicitly takes into the account both observational and modeling errors. The quality of the velocity reconstruction was validated against independent bottom-mounted ADCP data, the background model evolution, and against the results of spatial interpolation by Kriging technique. All tests demonstrated significant (30 to 60 %) reduction of the model-data misfit for the velocity field obtained as a result of space-time optimal interpolation. Although the method was applied to recover surface circulation, it can be extended for assessment of the full 4D tidal flow dynamics using the data recorded throughout the entire water column.
C1 [Sentchev, Alexei] Univ Lille, Univ Littoral Cote Opale, CNRS, UMR LOG 8187, F-59000 Lille, France.
[Yaremchuk, Max] Stennis Space Ctr, Naval Res Lab, Mississippi, MS 39529 USA.
RP Sentchev, A (reprint author), Univ Lille, Univ Littoral Cote Opale, CNRS, UMR LOG 8187, F-59000 Lille, France.
EM Alexei.Sentchev@univ-littoral.fr; max.yaremchuk@nrlssc.navy.mil
FU Interreg IVB (NW Europe) "Pro-Tide" Program; US Office of Naval Research
FX The authors would like to acknowledge the support of the Interreg IVB
(NW Europe) "Pro-Tide" Program and support from the US Office of Naval
Research. The skill and experience of skipper Eric Lecuyer and his help
during the fieldwork are appreciated and acknowledged. We also thank two
anonymous reviewers for their valuable comments on the manuscript.
NR 36
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U1 1
U2 6
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1616-7341
EI 1616-7228
J9 OCEAN DYNAM
JI Ocean Dyn.
PD JAN
PY 2016
VL 66
IS 1
BP 119
EP 132
DI 10.1007/s10236-015-0913-z
PG 14
WC Oceanography
SC Oceanography
GA DA5BY
UT WOS:000367818300009
ER
PT J
AU Yaremchuk, M
Martin, P
Koch, A
Beattie, C
AF Yaremchuk, Max
Martin, Paul
Koch, Andrey
Beattie, Christopher
TI Comparison of the adjoint and adjoint-free 4dVar assimilation of the
hydrographic and velocity observations in the Adriatic Sea
SO OCEAN MODELLING
LA English
DT Article
DE Data assimilation; Ajoint analysis; Regional modeling
ID VARIATIONAL DATA ASSIMILATION; GENERAL-CIRCULATION MODEL; COASTAL OCEAN
MODEL; PART I; SENSITIVITY-ANALYSIS; THEORETICAL ASPECTS; DIFFUSION
OPERATOR; NAVDAS-AR; FORMULATION; SYSTEM
AB Performance of the adjoint and adjoint-free 4-dimensional variational (4dVar) data assimilation techniques is compared in application to the hydrographic surveys and velocity observations collected in the Adriatic Sea in 2006. Assimilating the data into the Navy Coastal Ocean Model (NCOM) has shown that both methods deliver similar reduction of the cost function and demonstrate comparable forecast skill at approximately the same computational expense. The obtained optimal states were, however, significantly different in terms of distance from the background state: application of the adjoint method resulted in a 30-40% larger departure, mostly due to the excessive level of ageostrophic motions in the southern basin of the Sea that was not covered by observations. Published by Elsevier Ltd.
C1 [Yaremchuk, Max; Martin, Paul] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS 39572 USA.
[Koch, Andrey] Univ So Mississippi, Dept Marine Sci, Hattiesburg, MS 39406 USA.
[Beattie, Christopher] Virginia Tech, Dept Math, Blacksburg, VA USA.
RP Yaremchuk, M (reprint author), Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS 39572 USA.
EM max.yaremchuk@nrlssc.navy.mil
RI Beattie, Christopher/B-2191-2017
OI Beattie, Christopher/0000-0003-3302-4845
FU Office of Naval Research [61153N]; Einstein Foundation of Berlin; NSF
[DMS-1217156]
FX The authors were supported by the Office of Naval Research under program
element 61153N "Adjoint-free 4dVar for Ocean Models". The work of C.
Beattie was additionally supported in part by the Einstein Foundation of
Berlin and the NSF through Grant DMS-1217156. We gratefully acknowledge
P. Sakaulakis for help with parallelization issues and M. Carrier and S.
Smith for their kind assistance in configuring the NCOM 4dVar data
assimilation system. Helpful discussions with I. Shulman are also
acknowledged.
NR 53
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Z9 0
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1463-5003
EI 1463-5011
J9 OCEAN MODEL
JI Ocean Model.
PD JAN
PY 2016
VL 97
BP 129
EP 140
DI 10.1016/j.ocemod.2015.10.010
PG 12
WC Meteorology & Atmospheric Sciences; Oceanography
SC Meteorology & Atmospheric Sciences; Oceanography
GA DA1LB
UT WOS:000367556200009
ER
PT J
AU Peteet, DM
Nichols, JE
Moy, CM
McGeachy, A
Perez, M
AF Peteet, Dorothy M.
Nichols, Jonathan E.
Moy, Christopher M.
McGeachy, Alicia
Perez, Max
TI Recent and Holocene climate change controls on vegetation and carbon
accumulation in Alaskan coastal muskegs
SO QUATERNARY SCIENCE REVIEWS
LA English
DT Article
DE Pollen; Macrofossils; Carbon; Vegetation; Alaska; Alnus
ID SOUTH-CENTRAL ALASKA; LATE WISCONSIN GLACIATION; NORTH PACIFIC COAST;
GLACIER FLUCTUATIONS; RIVER DELTA; HISTORY; PEATLANDS; POLLEN; PEAT; BOG
AB Pollen, spore, macrofossil and carbon data from a peatland near Cordova, Alaska, reveal insights into the climate-vegetation-carbon interactions from the initiation of the Holocene, c. the last 11.5 ka, to the present (1 ka = 1000 calibrated years before present where 0 = 1950 CE). The Holocene period is characterized by early deposition of gyttja in a pond environment with aquatics such as Nuphar polysepalum and Potamogeton, and a significant regional presence of Alnus crispa subsp. sinuata. Carbon accumulation (50 g/m(2)/a) was high for a short interval in the early Holocene when Sphagnum peat accumulated, but was followed by a major decline to 13 g/m(2)/a from 7 to 3.7 ka when Cyperaceae and ericads such as Rhododendron (formerly Ledum) groenlandicum expanded. This shift to sedge growth is representative of many peatlands throughout the south-central region of Alaska, and indicates a drier, more evaporative environment with a large decline in carbon storage. The subsequent return to Sphagnum peat after 4 ka in the Neoglacial represents a widespread shift to moister, cooler conditions, which favored a resurgence of ericads, such as Andromeda polifolia, and increased carbon accumulation rate. The sustained Alnus expansion visible in the top 10 cm of the peat profile is correlative with glacial retreat and warming of the region in the last century, and suggests this colonization will continue as temperature increases and ice melts. Published by Elsevier Ltd.
C1 [Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Peteet, Dorothy M.; Nichols, Jonathan E.] Lamont Doherty Earth Observ, Palisades, NY USA.
[Moy, Christopher M.] Univ Otago, Dept Geol, Dunedin, New Zealand.
[McGeachy, Alicia] Spelman Coll, Atlanta, GA 30314 USA.
[Perez, Max] SUNY Binghamton, Binghamton, NY USA.
RP Peteet, DM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM peteet@ldeo.columbia.edu
OI Nichols, Jonathan/0000-0003-3913-2206
FU NSF ARC [1022979]; Climate Center of the Lamont Doherty Earth
Observatory; NASA Postdoctoral Program; US Geological Survey Mendenhall
Postdoctoral fellowship
FX This work is supported by NSF ARC #1022979 and the Climate Center of the
Lamont Doherty Earth Observatory. The Prince William Sound Science
Center in Cordova, Alaska, provided critical logistical support while
collecting the Corser Bog core as well as area orthophotos and other
geographical data. JEN and CMM also gratefully acknowledge support from
the NASA Postdoctoral Program and the US Geological Survey Mendenhall
Postdoctoral fellowship, respectively. We thank the reviewers for
constructive comments. This is LDEO contribution number.
NR 52
TC 1
Z9 1
U1 7
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-3791
J9 QUATERNARY SCI REV
JI Quat. Sci. Rev.
PD JAN 1
PY 2016
VL 131
BP 168
EP 178
DI 10.1016/j.quascirev.2015.10.032
PN A
PG 11
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA DA0MC
UT WOS:000367490200011
ER
PT J
AU Demosthenous, E
Borghesi, G
Mastorakos, E
Cant, RS
AF Demosthenous, Elena
Borghesi, Giulio
Mastorakos, Epaminondas
Cant, Robert Stewart
TI Direct Numerical Simulations of premixed methane flame initiation by
pilot n-heptane spray autoignition
SO COMBUSTION AND FLAME
LA English
DT Article
DE Dual fuel combustion; Autoignition; n-Heptane spray; Premixed methane;
Propagation
ID COMPRESSION IGNITION ENGINE; CONDITIONAL MOMENT CLOSURE; LOW-TEMPERATURE
COMBUSTION; COMPLEX CHEMISTRY DNS; DUAL FUEL ENGINE; NATURAL-GAS;
TURBULENT SPRAYS; SPARK-IGNITION; EMISSION CHARACTERISTICS; MIXING
LAYERS
AB Autoignition of n-heptane sprays in a methane/air mixture and the subsequent methane premixed flame ignition, a constant volume configuration relevant to pilot-ignited dual fuel engines, was investigated by DNS. It was found that reducing the pilot fuel quantity, increases its autoignition time. This is attributed to the faster disappearance of the most reactive mixture fraction (predicted from homogeneous reactor calculations) which is quite rich. Consequently, ignition of the n-heptane occurs at leaner mixtures. The premixed methane flame is eventually ignited due to heating gained by the pressure rise caused by the n-heptane oxidation, and heat and mass transfer of intermediates from the n-heptane autoignition kernels. For large amounts of the pilot fuel, the combustion of the n-heptane results in significant adiabatic compression of the methane-air mixture. Hence the slow methane oxidation is accelerated and is further promoted by the presence of species in the oxidizer stream originating from the already ignited regions. For small amounts of the pilot fuel intermediates reach the oxidizer stream faster due to the very lean mixtures surrounding the n-heptane ignition kernels. Therefore, the premixed methane oxidation is initiated at intermediate temperatures. Depending on the amount of n-heptane, different statistical behaviour of the methane oxidation is observed when this is investigated in a reaction progress variable space. In particular for large amounts of n-heptane the methane oxidation follows roughly an autoignition regime, whereas for small amounts of n-heptane methane oxidation is similar to a canonical premixed flame. The data can be used for validation of various turbulent combustion models for dual-fuel combustion. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Demosthenous, Elena; Mastorakos, Epaminondas; Cant, Robert Stewart] Univ Cambridge, Dept Engn, Hopkinson Lab, Cambridge CB2 1PZ, England.
[Borghesi, Giulio] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Demosthenous, E (reprint author), Univ Cambridge, Dept Engn, Hopkinson Lab, Cambridge CB2 1PZ, England.
EM ed398@cam.ac.uk
OI Mastorakos, Epaminondas/0000-0001-8245-5188
FU EPSRC [EP/J021997/1]
FX The computational costs for this work were covered by the EPSRC project
ref. no. EP/J021997/1.
NR 57
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U1 6
U2 17
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD JAN
PY 2016
VL 163
BP 122
EP 137
DI 10.1016/j.combustflame.2015.09.013
PG 16
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CZ7KP
UT WOS:000367278600011
ER
PT J
AU Bhattacharjee, S
Simsek, A
Olson, S
Ferkul, P
AF Bhattacharjee, Subrata
Simsek, Aslihan
Olson, Sandra
Ferkul, Paul
TI The critical flow velocity for radiative extinction in opposed-flow
flame spread in a microgravity environment: A comparison of
experimental, computational, and theoretical results
SO COMBUSTION AND FLAME
LA English
DT Article
DE Flame spread; Microgravity; Flammability; Extinction velocity; Radiative
extinction; Space station
ID QUIESCENT; FUELS
AB The effect of opposing flow on flame spread rate over thin solid fuel is investigated with the help of scaling theory, a comprehensive computational model, and experiments conducted aboard the International Space Station. While spread rate over thin fuels is independent of the opposing flow velocity in the thermal regime, in the microgravity regime, where the opposing flow can be very mild or even completely absent in the absence of buoyancy induced flow, the spread rate is known to decrease as the opposed flow is reduced. Under certain conditions, this can lead to flame extinguishment at a low enough flow velocity. This paper combines scaling arguments with computational results to predict a critical flow velocity for such flame extinction. Results from the recently conducted limited number of space based tests, presented in this paper, seem to confirm the prediction validating the closed-form formula for the critical extinction velocity. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Bhattacharjee, Subrata; Simsek, Aslihan] San Diego State Univ, Mech Engn, San Diego, CA 92182 USA.
[Olson, Sandra; Ferkul, Paul] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Bhattacharjee, S (reprint author), San Diego State Univ, Mech Engn, San Diego, CA 92182 USA.
EM prof.bhattacharjee@gmail.com
OI Ferkul, Paul/0000-0001-7655-2125; Simsek, Aslihan/0000-0003-0539-5294
FU NASA ISS Research Project Office
FX This work was funded by the NASA ISS Research Project Office with Dr.
David Urban serving as the contract monitor. We want to acknowledge the
invaluable assistance of astronauts Reid Wiseman and Alex Gerst, who ran
these BASS-II experiments. This work couldn't have been done without the
intense efforts of the BASS ops team (Jay Owens, Chuck Bunnell, Tibor
Lorik, and Carol Reynolds). We also want to acknowledge the NASA ground
support teams at GRC, JSC, and MSFC that supported the BASS-II
operations.
NR 20
TC 1
Z9 1
U1 1
U2 7
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD JAN
PY 2016
VL 163
BP 472
EP 477
DI 10.1016/j.combustflame.2015.10.023
PG 6
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CZ7KP
UT WOS:000367278600038
ER
PT J
AU Martin, R
AF Martin, Rodney
TI The Influence of System Stability and Dynamics on the Accuracy of
Level-Crossing Prediction
SO IEEE TRANSACTIONS ON AUTOMATIC CONTROL
LA English
DT Article
DE Alarm systems; fault detection; Kalman filtering; prediction problems
and methods; stability of linear systems
ID GAUSSIAN-PROCESSES
AB This technical note investigates the effect of stability on the probability of correctly predicting level-crossings for the output of a linear dynamical system driven by Gaussian noise. It is found that decreasing the stability margin has a favorable effect on predictive capability. The insight from this finding was derived from a parametric analysis of a given measure of predictive capability, represented as an explicit function of the spectral radius. The formulae used to characterize this relationship were derived under strict technical conditions in previous work. However, as a result of the closed-form nature of these expressions, using these formulae to gain insight on the influence of stability was much more computationally efficient than would otherwise be possible under more relaxed technical conditions. These findings are also extended to determine how system dynamics are concurrently influenced, as quantified by both the natural frequency and damping ratio of a second order linear dynamical system. It is found that for an optimal predictor, as the stability margin is decreased infinitesimally, system dynamics have no adverse influence on one-step zero-crossing predictive capability. However, for two suboptimal predictors investigated it is found that under the same conditions the system dynamics influence predictive capability adversely as the natural frequency approach critical values. For zero-crossing predictive capability with a prediction horizon consisting of a single step, these facts will be rigorously proven for any ARMA(2,1) process.
C1 [Martin, Rodney] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Martin, R (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
EM rodney.martin@nasa.gov
NR 9
TC 0
Z9 0
U1 4
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9286
EI 1558-2523
J9 IEEE T AUTOMAT CONTR
JI IEEE Trans. Autom. Control
PD JAN
PY 2016
VL 61
IS 1
BP 264
EP 269
DI 10.1109/TAC.2015.2434033
PG 6
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA CZ7ND
UT WOS:000367285200029
ER
PT J
AU Toure, AM
Rodell, M
Yang, ZL
Beaudoing, H
Kim, E
Zhang, YF
Kwon, YW
AF Toure, Ally M.
Rodell, Matthew
Yang, Zong-Liang
Beaudoing, Hiroko
Kim, Edward
Zhang, Yongfei
Kwon, Yonghwan
TI Evaluation of the Snow Simulations from the Community Land Model,
Version 4 (CLM4)
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Models and modeling; Land surface model; Model errors
ID INTERACTIVE MULTISENSOR SNOW; WESTERN UNITED-STATES; ICE MAPPING SYSTEM;
WATER EQUIVALENT; COVER VARIABILITY; NORTH-AMERICA; MODIS; CLIMATE;
DEPTH; PRECIPITATION
AB This paper evaluates the simulation of snow by the Community Land Model, version 4 (CLM4), the land model component of the Community Earth System Model, version 1.0.4 (CESM1.0.4). CLM4 was run in an offline mode forced with the corrected land-only replay of the Modern-Era Retrospective Analysis for Research and Applications (MERRA-Land) and the output was evaluated for the period from January 2001 to January 2011 over the Northern Hemisphere poleward of 30 degrees N. Simulated snow-cover fraction (SCF), snow depth, and snow water equivalent (SWE) were compared against a set of observations including the Moderate Resolution Imaging Spectroradiometer (MODIS) SCF, the Interactive Multisensor Snow and Ice Mapping System (IMS) snow cover, the Canadian Meteorological Centre (CMC) daily snow analysis products, snow depth from the National Weather Service Cooperative Observer (COOP) program, and Snowpack Telemetry (SNOTEL) SWE observations. CLM4 SCF was converted into snow-cover extent (SCE) to compare with MODIS SCE. It showed good agreement, with a correlation coefficient of 0.91 and an average bias of -1.54 x 10(2) km(2). Overall, CLM4 agreed well with IMS snow cover, with the percentage of correctly modeled snow-no snow being 94%. CLM4 snow depth and SWE agreed reasonably well with the CMC product, with the average bias (RMSE) of snow depth and SWE being 0.044 m (0.19 m) and -0.010 m (0.04 m), respectively. CLM4 underestimated SNOTEL SWE and COOP snow depth. This study demonstrates the need to improve the CLM4 snow estimates and constitutes a benchmark against which improvement of the model through data assimilation can be measured.
C1 [Toure, Ally M.; Rodell, Matthew; Beaudoing, Hiroko; Kim, Edward] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Toure, Ally M.] Univ Space Res Assoc, Columbia, MD USA.
[Yang, Zong-Liang; Zhang, Yongfei; Kwon, Yonghwan] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX USA.
[Beaudoing, Hiroko] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Rodell, M (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Code 617,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM matthew.rodell@nasa.gov
RI Yang, Zong-Liang/B-4916-2011; Rodell, Matthew/E-4946-2012
OI Rodell, Matthew/0000-0003-0106-7437
FU NASA's Science of Terra and Aqua program
FX This study is funded by NASA's Science of Terra and Aqua program.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center. Thanks go to K. R. Arsenault for
preprocessing SNOTEL and COOP data. Thanks also go to Sam Lewis and
Keith Oleson at NCAR for their help in setting up and running CESM on
NASA Center for Climate Simulation (NCCS) computers.
NR 78
TC 2
Z9 2
U1 0
U2 18
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JAN
PY 2016
VL 17
IS 1
BP 153
EP 170
DI 10.1175/JHM-D-14-0165.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9FL
UT WOS:000367403100001
ER
PT J
AU Behrangi, A
Guan, B
Neiman, PJ
Schreier, M
Lambrigtsen, B
AF Behrangi, Ali
Guan, Bin
Neiman, Paul J.
Schreier, Mathias
Lambrigtsen, Bjorn
TI On the Quantification of Atmospheric Rivers Precipitation from Space:
Composite Assessments and Case Studies over the Eastern North Pacific
Ocean and the Western United States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Physical Meteorology and Climatology; Hydrology; Hydrometeorology;
Observational techniques and algorithms; Remote sensing; Satellite
observations; Flood events; IPWG-7
ID SIERRA-NEVADA; EXTREME PRECIPITATION; PASSIVE MICROWAVE; CALIFORNIA;
SATELLITE; RAIN; COAST; ALGORITHM; LAND; CLIMATE
AB Atmospheric rivers (ARs) are often associated with extreme precipitation, which can lead to flooding or alleviate droughts. A decade (2003-12) of landfalling ARs impacting the North American west coast (between 32.5 degrees and 52.5 degrees N) is collected to assess the skill of five commonly used satellite-based precipitation products [T3B42, T3B42 real-time (T3B42RT), CPC morphing technique (CMORPH), PERSIANN, and PERSIANN-Cloud Classification System (CCS)] in capturing ARs' precipitation rate and pattern. AR detection was carried out using a database containing twice-daily satellite-based integrated water vapor composite observations. It was found that satellite products are more consistent over ocean than land and often significantly underestimate precipitation rate over land compared to ground observations. Incorrect detection of precipitation from IR-based methods is prevalent over snow and ice surfaces where microwave estimates often show underestimation or missing data. Bias adjustment using ground observation is found very effective to improve satellite products, but it also raises concern regarding near-real-time applicability of satellite products for ARs. The analysis using individual case studies (6-8 January and 13-14 October 2009) and an ensemble of AR events suggests that further advancement in capturing orographic precipitation and precipitation over cold and frozen surfaces is needed to more reliably quantify AR precipitation from space.
C1 [Behrangi, Ali; Guan, Bin; Schreier, Mathias; Lambrigtsen, Bjorn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Neiman, Paul J.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91109 USA.
EM ali.behrangi@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
FU NASA New Investigator Program (NIP), Energy and Water Cycle Study
(NEWS); National Aeronautics and Space Administration; Weather program
awards
FX 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.
Financial support is also made available from NASA New Investigator
Program (NIP), Energy and Water Cycle Study (NEWS), and Weather program
awards. Government sponsorship is acknowledged.
NR 50
TC 1
Z9 1
U1 2
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JAN
PY 2016
VL 17
IS 1
BP 369
EP 382
DI 10.1175/JHM-D-15-0061.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9GF
UT WOS:000367405100001
ER
PT J
AU Kidd, C
Matsui, T
Chern, J
Mohr, K
Kummerow, C
Randel, D
AF Kidd, Chris
Matsui, Toshihisa
Chern, Jiundar
Mohr, Karen
Kummerow, Chris
Randel, Dave
TI Global Precipitation Estimates from Cross-Track Passive Microwave
Observations Using a Physically Based Retrieval Scheme
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Atm; Ocean Structure; Phenomena; Precipitation; Rainfall; Physical
Meteorology and Climatology; Radiances; Observational techniques and
algorithms; Microwave observations; Satellite observations; Models and
modeling; Cloud resolving models; IPWG-7
ID NUMERICAL WEATHER PREDICTION; PROFILING ALGORITHM GPROF; RAINFALL
ESTIMATION; PART II; MODEL; SYSTEM; RADAR; INFORMATION; FREQUENCIES;
FRAMEWORK
AB The estimation of precipitation across the globe from satellite sensors provides a key resource in the observation and understanding of our climate system. Estimates from all pertinent satellite observations are critical in providing the necessary temporal sampling. However, consistency in these estimates from instruments with different frequencies and resolutions is critical. This paper details the physically based retrieval scheme to estimate precipitation from cross-track (XT) passive microwave (PM) sensors on board the constellation satellites of the Global Precipitation Measurement (GPM) mission. Here the Goddard profiling algorithm (GPROF), a physically based Bayesian scheme developed for conically scanning (CS) sensors, is adapted for use with XT PM sensors. The present XT GPROF scheme utilizes a model-generated database to overcome issues encountered with an observational database as used by the CS scheme. The model database ensures greater consistency across meteorological regimes and surface types by providing a more comprehensive set of precipitation profiles. The database is corrected for bias against the CS database to ensure consistency in the final product. Statistical comparisons over western Europe and the United States show that the XT GPROF estimates are comparable with those from the CS scheme. Indeed, the XT estimates have higher correlations against surface radar data, while maintaining similar root-mean-square errors. Latitudinal profiles of precipitation show the XT estimates are generally comparable with the CS estimates, although in the southern midlatitudes the peak precipitation is shifted equatorward while over the Arctic large differences are seen between the XT and the CS retrievals.
C1 [Kidd, Chris; Matsui, Toshihisa; Chern, Jiundar] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kidd, Chris; Matsui, Toshihisa; Chern, Jiundar; Mohr, Karen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kummerow, Chris; Randel, Dave] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Kidd, C (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20771 USA.
EM chris.kidd@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA-University of Maryland Master [526697/T613]
FX Funding for this research is made possible through the NASA-University
of Maryland Master Grant 526697/T613. The authors wish to thank NSSL and
CEDA for the provision of the surface datasets and the GPM PPS team for
provision of the satellite datasets.
NR 48
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U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JAN
PY 2016
VL 17
IS 1
BP 383
EP 400
DI 10.1175/JHM-D-15-0051.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9GF
UT WOS:000367405100002
ER
PT J
AU Li, YJ
Stier, B
Bednarcyk, B
Simon, JW
Reese, S
AF Li, Yujun
Stier, Bertram
Bednarcyk, Brett
Simon, Jaan-Willem
Reese, Stefanie
TI The effect of fiber misalignment on the homogenized properties of
unidirectional fiber reinforced composites
SO MECHANICS OF MATERIALS
LA English
DT Article
DE Unidirectional composites; Fiber misalignment; Orientation distribution
function; Microsphere; Homogenization
ID SPHERE; DEFORMATION; ELASTICITY; BEHAVIOR; MODELS
AB Unidirectional fiber-reinforced composites have been widely used over the past several decades in industry due to their high specific strength and superior fatigue characteristics. In order to predict their overall mechanical properties, typically, a homogenization procedure is used to relate the constituent properties and the macroscopic behavior, in which the representative one-dimensional material description is generalized to a fully three-dimensional constitutive model. The aim of this study is primarily to understand the influence of fiber misalignment on the effective composite material properties. In order to achieve this, a microsphere based homogenization approach is proposed, in which the passage from microstructural contributions to the macroscopic response is obtained by integration over the surface of a unit microsphere. The result is compared with a micromechanically motivated model and the High-Fidelity Generalized Method of Cells model. The results illustrate the effects of the fiber misalignment degree in terms of the concentration dependence of the predicted overall properties. From these findings, elastic properties can be obtained for the design of composite structures. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Li, Yujun; Stier, Bertram; Simon, Jaan-Willem; Reese, Stefanie] Rhein Westfal TH Aachen, Inst Appl Mech, D-52074 Aachen, Germany.
[Bednarcyk, Brett] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Li, YJ (reprint author), Rhein Westfal TH Aachen, Inst Appl Mech, Mies van der Rohe Str 1, D-52074 Aachen, Germany.
EM yujun.li@rwth-aachen.de
RI Yujun, LI/H-5043-2013; Simon, Jaan/J-9114-2014
OI Simon, Jaan/0000-0003-2231-2569
FU China Scholarship Council (CSC); Deutsche Forschungsgemeinschaft (DFG)
[Si 1959/2-1]; Exploratory Research Space (ERS) of RWTH Aachen
University
FX The first author gratefully acknowledges the financial support of the
China Scholarship Council (CSC).; The authors Brett Bednarcyk and
Jaan-Willem Simon gratefully acknowledge support from the Deutsche
Forschungsgemeinschaft (DFG) grant no. Si 1959/2-1 and the
Theodore-von-Karman Fellowship of the Exploratory Research Space (ERS)
of RWTH Aachen University, who made this collaboration possible.
NR 34
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U1 6
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6636
EI 1872-7743
J9 MECH MATER
JI Mech. Mater.
PD JAN
PY 2016
VL 92
BP 261
EP 274
DI 10.1016/j.mechmat.2015.10.002
PG 14
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA CZ7KZ
UT WOS:000367279600021
ER
PT J
AU Brown, ME
Ihli, M
Hendrick, O
Delgado-Arias, S
Escobar, VM
Griffith, P
AF Brown, Molly E.
Ihli, Monica
Hendrick, Oscar
Delgado-Arias, Sabrina
Escobar, Vanessa M.
Griffith, Peter
TI Social network and content analysis of the North American Carbon Program
as a scientific community of practice
SO SOCIAL NETWORKS
LA English
DT Article
DE North American Carbon Program; Carbon cycle; Knowledge domain; Knowledge
visualization; Communities of practice; Co-authorship network analysis
ID CLIMATE-CHANGE; SCIENCE; COLLABORATION; KNOWLEDGE; PATTERNS; HEALTH
AB The North American Carbon Program (NACP) was formed to further the scientific understanding of sources, sinks, and stocks of carbon in Earth's environment. Carbon cycle science integrates multidisciplinary research, providing decision-support information for managing climate and carbon-related change across multiple sectors of society. This investigation uses the conceptual framework of communities of practice (CoP) to explore the role that the NACP has played in connecting researchers into a carbon cycle knowledge network, and in enabling them to conduct physical science that includes ideas from social science. A CoP describes the communities formed when people consistently engage in shared communication and activities toward a common passion or learning goal. We apply the CoP model by using keyword analysis of abstracts from scientific publications to analyze the research outputs of the NACP in terms of its knowledge domain. We also construct a co-authorship network from the publications of core NACP members, describe the structure and social pathways within the community. Results of the content analysis indicate that the NACP community of practice has substantially expanded its research on human and social impacts on the carbon cycle, contributing to a better understanding of how human and physical processes interact with one another. Results of the co-authorship social network analysis demonstrate that the NACP has formed a tightly connected community with many social pathways through which knowledge may flow, and that it has also expanded its network of institutions involved in carbon cycle research over the past seven years. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Brown, Molly E.] Univ Maryland, Dept Geog Sci, College Pk, MD 20740 USA.
[Ihli, Monica] Univ Tennessee, Knoxville, TN 37996 USA.
[Hendrick, Oscar; Delgado-Arias, Sabrina; Escobar, Vanessa M.; Griffith, Peter] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
RP Brown, ME (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20740 USA.
EM mbrown52@umd.edu
RI Brown, Molly/E-2724-2010; Griffith, Peter/I-1392-2016
OI Brown, Molly/0000-0001-7384-3314; Ihli, Monica/0000-0001-6907-6167;
Griffith, Peter/0000-0002-4267-7429
FU National Aeronautics and Space Administration through a grant under the
Carbon Monitoring System Science Area, Earth Science Directorate
FX This research was funded by the National Aeronautics and Space
Administration through a grant under the Carbon Monitoring System
Science Area, Earth Science Directorate. This study was part of the
North American Carbon Program.
NR 37
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U1 11
U2 26
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-8733
EI 1879-2111
J9 SOC NETWORKS
JI Soc. Networks
PD JAN
PY 2016
VL 44
BP 226
EP 237
DI 10.1016/j.socnet.2015.10.002
PG 12
WC Anthropology; Sociology
SC Anthropology; Sociology
GA CZ9NI
UT WOS:000367423900021
ER
PT J
AU Benafan, O
Noebe, RD
Halsmer, TJ
AF Benafan, O.
Noebe, R. D.
Halsmer, T. J.
TI Static rock splitters based on high temperature shape memory alloys for
planetary explorations
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Shape memory alloys; Rock splitting; NiTiHf; Geologic excavation;
Blocking force
AB A static rock splitter device based on high-force, high-temperature shape memory alloys (HTSMAs) was developed for space related applications requiring controlled geologic excavation in planetary bodies such as the moon, Mars, and near-Earth asteroids. The device, hereafter referred to as the shape memory alloy rock splitter (SMARS), consisted of active (expanding) elements made of Ni50.3Ti29.7Hf20 (at%) that generate extremely large forces in response to thermal input. The pre-shaping (training) of these elements was accomplished using isothermal, isobaric and cyclic training methods, which resulted in active components capable of generating stresses in excess of 1.5 GPa. The corresponding strains (or displacements) were also evaluated and were found to be 2-3%, essential to rock fracturing and/or splitting when placed in a borehole. SMARS performance was evaluated using a testbed consisting of a temperature controller, custom heaters and heater holders, and an enclosure for rock placement and breakage. The SMARS system was evaluated using various rock types including igneous rocks (e.g., basalt, quartz, granite) and sedimentary rocks (e.g., sandstone, limestone). (C) 2015 Published by Elsevier Ltd. on behalf of IAA.
C1 [Benafan, O.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Halsmer, T. J.] Jacobs Technol, Cleveland, OH 44135 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov
FU NASA Space Technology Mission Directorate (STMD), Center Innovation Fund
(CIF)
FX Funding from the NASA Space Technology Mission Directorate (STMD),
Center Innovation Fund (CIF) is gratefully acknowledged. Manufacturing
and imaging support from Grant E. Feichter, D.J. Brinkman, B.R. Caswell,
and D. Brown are gratefully acknowledged. Material development support
from (ARMD) Transformational Tools & Technologies (TTT) project is
gratefully acknowledged. The authors thank S.A. Padula II, G.S. Bigelow,
A. Garg, and D.J. Gaydosh, (shape memory alloy team) for helpful
discussions. The authors also thank C.M. Creager and P.B. Abel for
support in the SLOPE facility.
NR 47
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U1 6
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD JAN-FEB
PY 2016
VL 118
BP 137
EP 157
DI 10.1016/j.actaastro.2015.10.009
PG 21
WC Engineering, Aerospace
SC Engineering
GA CZ1NQ
UT WOS:000366873000013
ER
PT J
AU Wichman, IS
Olson, SL
Miller, FJ
Hariharan, A
AF Wichman, Indrek S.
Olson, Sandra L.
Miller, Fletcher J.
Hariharan, Ashwin
TI Fire in Microgravity
SO AMERICAN SCIENTIST
LA English
DT Article
ID MODEL
C1 [Wichman, Indrek S.] Michigan State Univ, Mech Engn, Energy & Automot Res Labs, E Lansing, MI 48824 USA.
[Olson, Sandra L.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
[Miller, Fletcher J.] San Diego State Univ, Mech Engn, San Diego, CA 92182 USA.
[Hariharan, Ashwin] Michigan State Univ, E Lansing, MI 48824 USA.
RP Wichman, IS (reprint author), Michigan State Univ, Mech Engn, Energy & Automot Res Labs, E Lansing, MI 48824 USA.
EM wichman@egr.msu.edu
NR 4
TC 0
Z9 0
U1 4
U2 4
PU SIGMA XI-SCI RES SOC
PI RES TRIANGLE PK
PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA
SN 0003-0996
EI 1545-2786
J9 AM SCI
JI Am. Scientist
PD JAN-FEB
PY 2016
VL 104
IS 1
BP 44
EP 51
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CZ6JW
UT WOS:000367208400017
ER
PT J
AU Fan, YZ
Li, W
Voss, KJ
Gatebe, CK
Stamnes, K
AF Fan, Yongzhen
Li, Wei
Voss, Kenneth J.
Gatebe, Charles K.
Stamnes, Knut
TI Neural network method to correct bidirectional effects in water-leaving
radiance
SO APPLIED OPTICS
LA English
DT Article
ID ATMOSPHERE-OCEAN SYSTEM; DIFFUSE-REFLECTANCE; PHASE FUNCTION; CASE-1
WATERS; DETAILED VALIDATION; UPWELLING RADIANCE; RADIATIVE-TRANSFER;
LIGHT-SCATTERING; COASTAL; ABSORPTION
AB Ocean color algorithms that rely on "atmospherically corrected" nadir water-leaving radiances to infer information about marine constituents such as the chlorophyll concentration depend on a reliable method to convert the angle-dependent measured radiances from the observation direction to the nadir direction. It is also important to convert the measured radiances to the nadir direction when comparing and merging products from different satellite missions. The standard correction method developed by Morel and coworkers requires knowledge of the chlorophyll concentration. Also, the standard method was developed based on the Case 1 (open ocean) assumption, which makes it unsuitable for Case 2 situations such as turbid coastal waters. We introduce a neural network method to convert the angle-dependent water-leaving radiance (or the corresponding remote sensing reflectance) from the observation direction to the nadir direction. This method relies on neither an "atmospheric correction" nor prior knowledge of the water constituents or the inherent optical properties. It directly converts the remote sensing reflectance from an arbitrary slanted viewing direction to the nadir direction by using a trained neural network. This method is fast and accurate, and it can be easily adapted to different remote sensing instruments. Validation using NuRADS measurements in different types of water shows that this method is suitable for both Case 1 and Case 2 waters. In Case 1 or chlorophyll-dominated waters, our neural network method produces corrections similar to those of the standard method. In Case 2 waters, especially sediment-dominated waters, a significant improvement was obtained compared to the standard method. (C) 2015 Optical Society of America
C1 [Fan, Yongzhen; Li, Wei; Stamnes, Knut] Stevens Inst Technol, Light & Life Lab, Dept Phys & Engn Phys, Hoboken, NJ 07307 USA.
[Voss, Kenneth J.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Gatebe, Charles K.] NASAs, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fan, YZ (reprint author), Stevens Inst Technol, Light & Life Lab, Dept Phys & Engn Phys, Hoboken, NJ 07307 USA.
EM yfan@stevens.edu
RI Gatebe, Charles/G-7094-2011
OI Gatebe, Charles/0000-0001-9261-2239
FU National Aeronautics and Space Administration (NASA)
FX National Aeronautics and Space Administration (NASA).
NR 38
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U1 0
U2 10
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 1
PY 2016
VL 55
IS 1
BP 10
EP 21
DI 10.1364/AO.55.000010
PG 12
WC Optics
SC Optics
GA CZ4RW
UT WOS:000367091400002
PM 26835615
ER
PT J
AU Taylor, LA
Logvinova, AM
Howarth, GH
Liu, Y
Peslier, AH
Rossman, GR
Guan, YB
Chen, Y
Sobolev, NV
AF Taylor, Lawrence A.
Logvinova, Alla M.
Howarth, Geoffrey H.
Liu, Yang
Peslier, Anne H.
Rossman, George R.
Guan, Yunbin
Chen, Yang
Sobolev, Nikolay V.
TI Low water contents in diamond mineral inclusions: Proto-genetic origin
in a dry cratonic lithosphere
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE diamond inclusions; NAM water contents; protogenetic minerals in
diamonds; cratonic lithosphere
ID UDACHNAYA KIMBERLITE; PERIDOTITE XENOLITHS; SIBERIAN PLATFORM; MANTLE
XENOLITHS; SOUTH-AFRICA; OLIVINE; HYDROGEN; GARNET; DIFFUSION; OH
AB The mantle is the major reservoir of Earth's water, hosted within Nominally Anhydrous Minerals (NAMs) (e.g., Bell and Rossman, 1992; Peslier et al., 2010; Peslier, 2010; Nestola and Smyth, 2015), in the form of hydrogen bonded to the silicate's structural oxygen. From whence cometh this water? Is the water in these minerals representative of the Earth's primitive upper mantle or did it come from melting events linked to crustal formation or to more recent metasomatic/re-fertilization events? During diamond formation, NAMs are encapsulated at hundreds of kilometers depth within the mantle, thereby possibly shielding and preserving their pristine water contents from re-equilibrating with fluids and melts percolating through the lithospheric mantle. Here we show that the NAMs included in diamonds from six locales on the Siberian Craton contain measurable and variable H2O concentrations from 2 to 34 parts per million by weight (ppmw) in olivine, 7 to 276 ppmw in clinopyroxene, and 11-17 ppmw in garnets. Our results suggest that if the inclusions were in equilibrium with the diamond-forming fluid, the water fugacity would have been unrealistically low. Instead, we consider the H2O contents of the inclusions, shielded by diamonds, as pristine representatives of the residual mantle prior to encapsulation, and indicative of a protogenetic origin for the inclusions. Hydrogen diffusion in the diamond does not appear to have modified these values significantly. The H2O contents of NAMs in mantle xenoliths may represent some later metasomatic event(s), and are not always representative of most of the continental lithospheric mantle. Results from the present study also support the conclusions of Peslier et al. (2010) and Novella et al. (2015) that the dry nature of the SCLM of a craton may provide stabilization of its thickened continental roots. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Taylor, Lawrence A.; Howarth, Geoffrey H.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37966 USA.
[Logvinova, Alla M.; Sobolev, Nikolay V.] Russian Acad Sci, Siberian Branch, VS Sobolev Inst Geol & Mineral, Novosibirsk, Russia.
[Logvinova, Alla M.; Sobolev, Nikolay V.] Novosibirsk State Univ, Novosibirsk 630090, Russia.
[Howarth, Geoffrey H.] Univ Cape Town, Dept Geol Sci, ZA-7700 Rondebosch, South Africa.
[Liu, Yang; Chen, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Peslier, Anne H.] NASA, Lyndon B Johnson Space Ctr, Jacobs, JETS, Houston, TX 77058 USA.
[Rossman, George R.; Guan, Yunbin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Taylor, LA (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37966 USA.
EM lataylor@utk.edu
RI Sobolev, Nikolay/A-3850-2014;
OI Rossman, George/0000-0002-4571-6884; Taylor,
Lawrence/0000-0002-1313-7597
FU NSF [EAR-1144337, EAR-1523393, EAR-1118335, EAR-1322082]
FX Assistance of Allan Patchen with the electron microprobe analyses is
gratefully recognized. This study was aided by the constructive
encouragement of Prof. Thomas Stachel from the University of Alberta.
Insightful comments, suggestions, and constructive criticisms from our
many colleagues are sincerely acknowledged, particularly reviewer Prof.
Fabrizio Nestola and an anonymous reviewer. These required considerable
improvement to the manuscript. Associate Editor Prof. Bernard Marty is
thanked for his very efficient handling of this manuscript. Part of this
research was performed at Jet Propulsion Laboratory, which is managed by
California Institute of Technology under a contract with NASA. This
research was performed with the support of NSF grants to LAT
(EAR-1144337; EAR-1523393), AHP (EAR-1118335), and GRR (EAR-1322082) for
which we are thankful.
NR 50
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U1 4
U2 28
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JAN 1
PY 2016
VL 433
BP 125
EP 132
DI 10.1016/j.epsl.2015.10.042
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CZ5CP
UT WOS:000367120300013
ER
PT J
AU Sikder, S
Chen, XD
Hossain, F
Roberts, JB
Robertson, F
Shum, CK
Turk, FJ
AF Sikder, Safat
Chen, Xiaodong
Hossain, Faisal
Roberts, Jason B.
Robertson, Franklin
Shum, C. K.
Turk, Francis J.
TI Are General Circulation Models Ready for Operational Streamflow
Forecasting for Water Management in the Ganges and Brahmaputra River
Basins?
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; RESOURCES MANAGEMENT; ATMOSPHERIC BRIDGE;
CLIMATE-CHANGE; UNITED-STATES; PREDICTION; HYDROLOGY; SKILL; ENSO;
BANGLADESH
AB This study asks the question of whether GCMs are ready to be operationalized for streamflow forecasting in South Asian river basins, and if so, at what temporal scales and for which water management decisions are they likely to be relevant? The authors focused on the Ganges, Brahmaputra, and Meghna basins for which there is a gridded hydrologic model calibrated for the 2002-10 period. The North American Multimodel Ensemble (NMME) suite of eight GCM hindcasts was applied to generate precipitation forecasts for each month of the 1982-2012 (30 year) period at up to 6 months of lead time, which were then downscaled according to the bias-corrected statistical downscaling (BCSD) procedure to daily time steps. A global retrospective forcing dataset was used for this downscaling procedure. The study clearly revealed that a regionally consistent forcing for BCSD, which is currently unavailable for the region, is one of the primary conditions to realize reasonable skill in streamflow forecasting. In terms of relative RMSE (normalized by reference flow obtained from the global retrospective forcings used in downscaling), streamflow forecast uncertainty (RMSE) was found to be 38%-50% at monthly scale and 22%-35% at seasonal (3 monthly) scale. The Ganges River (regulated) experienced higher uncertainty than the Brahmaputra River (unregulated). In terms of anomaly correlation coefficient (ACC), the streamflow forecasting at seasonal (3 monthly) scale was found to have less uncertainty (>0.3) than at monthly scale (<0.25). The forecast skill in the Brahmaputra basin showed more improvement when the time horizon was aggregated from monthly to seasonal than the Ganges basin. Finally, the skill assessment for the individual seasons revealed that the flow forecasting using NMME data had less uncertainty during monsoon season (July-September) in the Brahmaputra basin and in postmonsoon season (October-December) in the Ganges basin. Overall, the study indicated that GCMs can have value for management decisions only at seasonal or annual water balance applications at best if appropriate historical forcings are used in downscaling. The take-home message of this study is that GCMs are not yet ready for prime-time operationalization for a wide variety of multiscale water management decisions for the Ganges and Brahmaputra River basins.
C1 [Sikder, Safat; Chen, Xiaodong; Hossain, Faisal] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
[Roberts, Jason B.; Robertson, Franklin] Univ Alabama, Natl Space Sci Technol Ctr, NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35899 USA.
[Shum, C. K.] Ohio State Univ, Div Geodet Sci, Sch Earth Sci, Columbus, OH 43210 USA.
[Shum, C. K.] Chinese Acad Sci, Inst Geodesy & Geophys, Wuhan, Peoples R China.
[Turk, Francis J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hossain, F (reprint author), Univ Washington, Dept Civil & Environm Engn, 201 More Hall,Box 352700, Seattle, WA 98195 USA.
EM fhossain@uw.edu
OI Chen, Xiaodong/0000-0002-3089-2260
FU NASA SERVIR Grant [NNX12AM85G]; NASA WATER Grant [NNX15AC63G]; NASA
SERVIR Applied Sciences Team; NASA SERVIR program; Chinese Academy of
Sciences/SAFEA International Partnership Program for Creative Research
Teams [KZZD-EW-TZ-05]
FX The first three authors, Safat Sikder, Xiaodong Chen, and Faisal Hossain
wish to acknowledge support of the following sources: NASA SERVIR Grant
(NNX12AM85G) and NASA WATER Grant (NNX15AC63G). Dr. J. B. Roberts and F.
R. Robertson acknowledge support through the NASA SERVIR Applied
Sciences Team. Authors Francis J. Turk and C K Shum were also supported
by the NASA SERVIR program. C. K. Shum is also partially supported by
the Chinese Academy of Sciences/SAFEA International Partnership Program
for Creative Research Teams (Grant KZZD-EW-TZ-05). We also would like to
acknowledge the NMME project and its archival and dissemination support
by NOAA, NSF, NASA, and DOE with the help of IRI personnel. All authors
gratefully acknowledge the detailed reviews of three anonymous reviewers
and the editor that significantly improved the quality of the
manuscript.
NR 51
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Z9 1
U1 2
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JAN
PY 2016
VL 17
IS 1
BP 195
EP 210
DI 10.1175/JHM-D-14-0099.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9FX
UT WOS:000367404300001
ER
PT J
AU Stillman, S
Zeng, XB
Bosilovich, MG
AF Stillman, Susan
Zeng, Xubin
Bosilovich, Michael G.
TI Evaluation of 22 Precipitation and 23 Soil Moisture Products over a
Semiarid Area in Southeastern Arizona
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; SATELLITE RAINFALL PRODUCTS; GLOBAL
PRECIPITATION; MICROWAVE RADIOMETERS; GAUGE OBSERVATIONS; UNITED-STATES;
MODEL; REANALYSIS; CLIMATE; VARIABILITY
AB Precipitation and soil moisture are rigorously measured or estimated from a variety of sources. Here, 22 precipitation and 23 soil moisture products are evaluated against long-term daily observed precipitation (Pobs) and July-September daily observationally constrained soil moisture (SM) datasets over a densely monitored 150 km(2) watershed in southeastern Arizona, United States. Gauge-radar precipitation products perform best, followed by reanalysis and satellite products, and the median correlations of annual precipitation from these three categories with Pobs are 0.83, 0.68, and 0.46, respectively. Precipitation results from phase 5 of the Coupled Model Intercomparison Project (CMIP5) are the worst, including an overestimate of cold season precipitation and a lack of significant correlation of annual precipitation with Pobs from all (except one) models. Satellite soil moisture products perform best, followed by land data assimilation systems and reanalyses, and the CMIP5 results are the worst. For instance, the median unbiased root-mean-square difference (RMSD) values of July-September soil moisture compared with SM are 0.0070, 0.011, 0.014, and 0.029 m(3) m(-3) for these four product categories, respectively. All 17 (except 3) precipitation [17 (except 2) soil moisture] products with at least 20 years of data agree with Pobs (SM) without significant trends. The uncertainties associated with the scale mismatch between Pobs and coarser-resolution products are addressed using two 4-km gauge-radar precipitation products, and their impact on the results presented in this study is overall small. These results identify strengths and weaknesses of each product for future improvement; they also emphasize the importance of using multiple gauge-radar and satellite products along with their uncertainties in evaluating reanalyses and models.
C1 [Stillman, Susan; Zeng, Xubin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA.
[Bosilovich, Michael G.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Stillman, S (reprint author), Univ Arizona, Dept Atmospher Sci, Phys Atmospher Sci Bldg,Rm 542,1118 E 4th St, Tucson, AZ 85721 USA.
EM sstill88@email.arizona.edu
RI Bosilovich, Michael/F-8175-2012;
OI Zeng, Xubin/0000-0001-7352-2764
FU NSF [EF-1238908, AGS-0944101]; NASA [NNX14AM02G]
FX This work was supported by NSF (EF-1238908 and AGS-0944101) and NASA
(NNX14AM02G). Two anonymous reviewers are thanked for helpful comments
that significantly increased the clarity of our presentation. The
USDA-ARS Southwest Watershed Research Center is thanked for providing
long-term, high-quality precipitation and soil moisture data used in
this study (available at http://www.tucson.ars.ag.gov/dap/). Several of
the datasets used in this analysis were obtained from the following
archives: NCAR Computational and Information Systems Laboratory;
Barcelona Expert Center; DOE Program for Climate Model Diagnosis and
Intercomparison; University of California, Irvine, Center for
Hydrometeorology and Remote Sensing; NOAA Earth System Research
Laboratory; NCAR Earth Observing Laboratory; National Snow and Ice Data
Center; NASA Goddard Earth Sciences Data and Information Services
Center; and Earth Online. We would like to acknowledge the archive
developers for providing high-quality data that made this work possible.
Additionally, we appreciate ECMWF and NASA for providing nicely
formatted data for public use.
NR 65
TC 2
Z9 2
U1 2
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD JAN
PY 2016
VL 17
IS 1
BP 211
EP 230
DI 10.1175/JHM-D-15-0007.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9FX
UT WOS:000367404300002
ER
PT J
AU Zhu, X
Yee, JH
Cai, M
Swartz, WH
Coy, L
Aquila, V
Garcia, R
Talaat, ER
AF Zhu, Xun
Yee, Jeng-Hwa
Cai, Ming
Swartz, William H.
Coy, Lawrence
Aquila, Valentina
Garcia, Rolando
Talaat, Elsayed R.
TI Diagnosis of Middle-Atmosphere Climate Sensitivity by the Climate
Feedback-Response Analysis Method
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID LOWER-STRATOSPHERIC TEMPERATURES; ANNUAL CYCLE; RADIATIVE BALANCE;
MESOSPHERE; CIRCULATION; PARAMETERIZATION; OZONE; WAVES; ACCELERATION;
TROPOSPHERE
AB The authors present a new method to diagnose the middle-atmosphere climate sensitivity by extending the climate feedback-response analysis method (CFRAM) for the coupled atmosphere-surface system to the middle atmosphere. The middle-atmosphere CFRAM (MCFRAM) is built on the atmospheric energy equation per unit mass with radiative heating and cooling rates as its major thermal energy sources. MCFRAM preserves CFRAM's unique feature of additivity, such that partial temperature changes due to variations in external forcing and feedback processes can be added to give a total temperature change for direct comparison with the observed temperature change. In addition, MCFRAM establishes a physical relationship of radiative damping between the energy perturbations associated with various feedback processes and temperature perturbations associated with thermal responses. In this study, MCFRAM is applied to both observations and model output fields to diagnose the middle-atmosphere climate sensitivity. The authors found that the largest component of the middle-atmosphere temperature response to the 11-yr solar cycle (solar maximum vs solar minimum) is the partial temperature change due to the variation of the solar flux. Increasing CO2 cools the middle atmosphere, whereas the partial temperature change due to changes in O-3 can be either positive or negative. The application of MCFRAM to model dynamical fields reconfirms the advantage of introducing the residual circulation to characterize middle-atmosphere dynamics in terms of the partial temperature changes. The radiatively driven globally averaged partial temperature change is approximately equal to the observed temperature change, ranging from -0.5 K near 25 km to -1.0 K near 70 km between solar maximum and solar minimum.
C1 [Zhu, Xun; Yee, Jeng-Hwa; Swartz, William H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Cai, Ming] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Coy, Lawrence] Sci Syst & Applicat Inc, Lanham, MD USA.
[Aquila, Valentina] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA.
[Aquila, Valentina] Johns Hopkins Univ, Baltimore, MD USA.
[Garcia, Rolando] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Talaat, Elsayed R.] NASA, Heliophys Div, Washington, DC 20546 USA.
RP Zhu, X (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM xun.zhu@jhuapl.edu
RI Aquila, Valentina/D-7267-2012; Zhu, Xun/C-2097-2016; Swartz,
William/A-1965-2010
OI Aquila, Valentina/0000-0003-2060-6694; Zhu, Xun/0000-0001-7860-6430;
Swartz, William/0000-0002-9172-7189
FU NASA Living With a Star Program [NNX13AF91G]; NASA Geospace Science
Program [NNX13AE33G]
FX This research was supported by NASA Living With a Star Program under
Grant NNX13AF91G and NASA Geospace Science Program under Grant
NNX13AE33G to The Johns Hopkins University Applied Physics Laboratory.
Comments on the manuscripts by three anonymous reviewers and by Jae N.
Lee are also appreciated.
NR 53
TC 1
Z9 1
U1 2
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JAN
PY 2016
VL 73
IS 1
BP 3
EP 23
DI 10.1175/JAS-D-15-0013.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ9CZ
UT WOS:000367396700001
ER
PT J
AU Norby, RJ
De Kauwe, MG
Domingues, TF
Duursma, RA
Ellsworth, DS
Goll, DS
Lapola, DM
Luus, KA
MacKenzie, AR
Medlyn, BE
Pavlick, R
Rammig, A
Smith, B
Thomas, R
Thonicke, K
Walker, AP
Yang, XJ
Zaehle, S
AF Norby, Richard J.
De Kauwe, Martin G.
Domingues, Tomas F.
Duursma, Remko A.
Ellsworth, David S.
Goll, Daniel S.
Lapola, David M.
Luus, Kristina A.
MacKenzie, A. Rob
Medlyn, Belinda E.
Pavlick, Ryan
Rammig, Anja
Smith, Benjamin
Thomas, Rick
Thonicke, Kirsten
Walker, Anthony P.
Yang, Xiaojuan
Zaehle, Soenke
TI Model-data synthesis for the next generation of forest free-air CO2
enrichment (FACE) experiments
SO NEW PHYTOLOGIST
LA English
DT Article
DE biodiversity; climate; elevated CO2; forest; free-air CO2 enrichment
(FACE); model-data synthesis; nitrogen (N); phosphorus (P)
ID ELEVATED ATMOSPHERIC CO2; TERRESTRIAL CARBON-CYCLE; WATER-USE
EFFICIENCY; TEMPERATE FOREST; ECOSYSTEM CARBON; STOMATAL CONDUCTANCE;
SEMIARID GRASSLAND; VEGETATION MODELS; DECIDUOUS FOREST; TROPICAL
FORESTS
AB The first generation of forest free-air CO2 enrichment (FACE) experiments has successfully provided deeper understanding about how forests respond to an increasing CO2 concentration in the atmosphere. Located in aggrading stands in the temperate zone, they have provided a strong foundation for testing critical assumptions in terrestrial biosphere models that are being used to project future interactions between forest productivity and the atmosphere, despite the limited inference space of these experiments with regards to the range of global ecosystems. Now, a new generation of FACE experiments in mature forests in different biomes and over a wide range of climate space and biodiversity will significantly expand the inference space. These new experiments are: EucFACE in a mature Eucalyptus stand on highly weathered soil in subtropical Australia; AmazonFACE in a highly diverse, primary rainforest in Brazil; BIFoR-FACE in a 150-yr-old deciduous woodland stand in central England; and SwedFACE proposed in a hemiboreal, Pinus sylvestris stand in Sweden. We now have a unique opportunity to initiate a model-data interaction as an integral part of experimental design and to address a set of cross-site science questions on topics including responses of mature forests; interactions with temperature, water stress, and phosphorus limitation; and the influence of biodiversity.
C1 [Norby, Richard J.; Walker, Anthony P.; Yang, Xiaojuan] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Norby, Richard J.; Walker, Anthony P.; Yang, Xiaojuan] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA.
[De Kauwe, Martin G.; Medlyn, Belinda E.] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia.
[Domingues, Tomas F.] Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Preto, Dept Biol, BR-14040901 Sao Paulo, Brazil.
[Duursma, Remko A.; Ellsworth, David S.; Medlyn, Belinda E.] Univ Western Sydney, Hawkesbury Inst Environm, Richmond, NSW 2751, Australia.
[Goll, Daniel S.] IPSL, Lab Sci Climat & Environnement, F-91198 Gif Sur Yvette, France.
[Lapola, David M.] Univ Estadual Paulista, Dept Ecol, Lab Ciencia Sistema Terrestre, BR-14800850 Sao Paulo, Brazil.
[Luus, Kristina A.; Zaehle, Soenke] Max Planck Inst Biogeochem, Biogeochem Integrat Dept, D-07701 Jena, Germany.
[MacKenzie, A. Rob; Thomas, Rick] Univ Birmingham, Birmingham Inst Forest Res, Birmingham B15 2TT, W Midlands, England.
[Pavlick, Ryan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rammig, Anja; Thonicke, Kirsten] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Rammig, Anja] Tech Univ Munich, TUM Sch Life Sci Weihenstephan, D-85354 Freising Weihenstephan, Germany.
[Smith, Benjamin] Lund Univ, Geocentrum 2, Dept Phys Geog & Ecosyst Sci, S-22362 Lund, Sweden.
RP Norby, RJ (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA.
EM rjn@ornl.gov
RI Norby, Richard/C-1773-2012; Domingues, Tomas/G-9707-2011; Yang,
Xiaojuan/I-3643-2016; Zaehle, Sonke/C-9528-2017; Walker,
Anthony/G-2931-2016; Smith, Benjamin/I-1212-2016
OI Norby, Richard/0000-0002-0238-9828; Domingues,
Tomas/0000-0003-2857-9838; Yang, Xiaojuan/0000-0002-2686-745X; Zaehle,
Sonke/0000-0001-5602-7956; Goll, Daniel/0000-0001-9246-9671; Walker,
Anthony/0000-0003-0557-5594; Smith, Benjamin/0000-0002-6987-5337
NR 90
TC 17
Z9 17
U1 19
U2 77
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 JAN
PY 2016
VL 209
IS 1
BP 17
EP 28
DI 10.1111/nph.13593
PG 12
WC Plant Sciences
SC Plant Sciences
GA CX0NM
UT WOS:000365393700006
PM 26249015
ER
PT J
AU Polozov, AG
Svensen, HH
Planke, S
Grishina, SN
Fristad, KE
Jerram, DA
AF Polozov, Alexander G.
Svensen, Henrik H.
Planke, Sverre
Grishina, Svetlana N.
Fristad, Kirsten E.
Jerram, Dougal A.
TI The basalt pipes of the Tunguska Basin (Siberia, Russia): High
temperature processes and volatile degassing into the end-Permian
atmosphere
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Tunguska Basin; Magma-brine interaction; Diatreme; End-Permian crisis;
Flood basalts; Large igneous province
ID TRIASSIC TRAP MAGMATISM; MASS EXTINCTION; PHREATOMAGMATIC EXPLOSIONS;
IRKUTSK AMPHITHEATER; SALIFEROUS ROCKS; MFCI EXPERIMENTS; CARBON-CYCLE;
PLATFORM; DEPOSITS; WATER
AB A number of mechanisms have been proposed to explain the end-Permian crisis. Many of them explore the link between this catastrophe and the Siberian Traps. We test the hypothesis that eruption of thermogenic gas generated in contact aureoles around igneous sills intruded into evaporite sequences of the Tunguska Basin triggered the crisis. In particular, we test the idea that the aspect that breccia pipes represent conduits for voluminous gas migration from the deep basins to the atmosphere. This contribution sheds new light on the pipe formation based on new field and borehole observations and electron microscopy analyses. Of more than three hundred mapped magnetite-bearing basalt pipes, 43 are classified as diatremes. The diatremes are usually circular or elliptical, with multiple zones of brecciation reaching the surface, sometimes with preserved in-filled crater lakes. The pipe diameter on the surface varies from a few tens of meters for small single diatremes to about a kilometer. The largest crater lake area is 2.7 km(2). We have conducted a detailed study of the breccias in the Sholokhovsk basalt pipe located within the Nepa potash deposit in the Tunguska Basin, Siberia, Russia (about N 59 degrees and E 107 degrees) and find that the breccias are cemented by carbonate matrix (calcite, dolomite) and halite. Breccia clasts are altered at various temperatures, evidenced by growth of albite and garnet from basaltic glass, and diopside, garnet, magnetite and chlorine-bearing amphibole (up to 1.8% Cl) in altered magmatic clasts. These mineral assemblages suggest high temperature interactions with evaporites within the pipe conduits. The large number of pipes support that degassing of halogen-rich volatiles was a widespread and violent process with implications for the end-Permian crisis. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Polozov, Alexander G.] Russian Acad Sci IGEM, Inst Geol Ore Deposits Petrog Mineral & Geochem, Moscow 119017, Russia.
[Polozov, Alexander G.; Svensen, Henrik H.; Planke, Sverre; Jerram, Dougal A.] Ctr Earth Evolut & Dynam, N-0315 Oslo, Norway.
[Planke, Sverre] Volcan Basin Petr Res AS VBPR, N-0349 Oslo, Norway.
[Grishina, Svetlana N.] RAS IGM SB, VS Sobolev Inst Geol & Mineral, Siberian Branch, Novosibirsk 630090, Russia.
[Fristad, Kirsten E.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Jerram, Dougal A.] DougalEARTH LTD, Solihull B91 3NU, W Midlands, England.
[Jerram, Dougal A.] Queensland Univ Technol, Earth Environm & Biol Sci, Brisbane, Qld 4001, Australia.
RP Polozov, AG (reprint author), Russian Acad Sci IGEM, Inst Geol Ore Deposits Petrog Mineral & Geochem, Staromonetnyi Side Str 35, Moscow 119017, Russia.
EM a.g.polozov@mail.ru
RI Polozov, Alexander/C-4221-2011
OI Polozov, Alexander/0000-0003-1422-4489
FU Norwegian Research Council via a SFF grants; CEED [223272]; Russian
Foundation for Basic Research [15-05-09345]
FX We gratefully acknowledge the financial support from the Norwegian
Research Council via a SFF grants to PGP and CEED (project number
223272, CEED), and a grant to H.H.S. (EPIC). A.G.P. with warmth keeps
the memory of Alexander E. Vorontsov, thesis supervisor who focused his
interest on the study of iron ore deposits in the Tunguska Basin, and
also thanks former colleagues from the Institute of Geochemistry in
Irkutsk. A.G.P. and S.N.G. acknowledge funding for completing of fluid
inclusion study from Russian Foundation for Basic Research grant to
S.N.G. (15-05-09345). M. Erambert assisted during EMP analyses. We would
like to thank Eric Font for editorial assistance and both anonymous
reviewers for their constructive comments.
NR 74
TC 5
Z9 5
U1 10
U2 27
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 JAN 1
PY 2016
VL 441
SI SI
BP 51
EP 64
DI 10.1016/j.palaeo.2015.06.035
PN 1
PG 14
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA CZ5AD
UT WOS:000367113600005
ER
PT J
AU Aschwanden, MJ
Crosby, NB
Dimitropoulou, M
Georgoulis, MK
Hergarten, S
McAteer, J
Milovanov, AV
Mineshige, S
Morales, L
Nishizuka, N
Pruessner, G
Sanchez, R
Sharma, AS
Strugarek, A
Uritsky, V
AF Aschwanden, Markus J.
Crosby, Norma B.
Dimitropoulou, Michaila
Georgoulis, Manolis K.
Hergarten, Stefan
McAteer, James
Milovanov, Alexander V.
Mineshige, Shin
Morales, Laura
Nishizuka, Naoto
Pruessner, Gunnar
Sanchez, Raul
Sharma, A. Surja
Strugarek, Antoine
Uritsky, Vadim
TI 25 Years of Self-Organized Criticality: Solar and Astrophysics
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Instabilities; Methods: statistical; Sun: flare; Stars: flare; Planets
and satellites: rings; Cosmic rays
ID X-RAY FLARES; ENERGETIC PARTICLE EVENTS; WAITING-TIME DISTRIBUTION;
CELLULAR-AUTOMATON MODEL; POWER-LAW DISTRIBUTION; CORONAL MASS
EJECTIONS; FOREST-FIRE MODEL; SPORADIC LOCALIZED RECONNECTIONS;
RENORMALIZATION-GROUP ANALYSIS; REGION TRANSIENT BRIGHTENINGS
AB Shortly after the seminal paper "Self-Organized Criticality: An explanation of 1/f noise" by Bak et al. (1987), the idea has been applied to solar physics, in "Avalanches and the Distribution of Solar Flares" by Lu and Hamilton (1991). In the following years, an inspiring cross-fertilization from complexity theory to solar and astrophysics took place, where the SOC concept was initially applied to solar flares, stellar flares, and magnetospheric substorms, and later extended to the radiation belt, the heliosphere, lunar craters, the asteroid belt, the Saturn ring, pulsar glitches, soft X-ray repeaters, blazars, black-hole objects, cosmic rays, and boson clouds. The application of SOC concepts has been performed by numerical cellular automaton simulations, by analytical calculations of statistical (powerlaw-like) distributions based on physical scaling laws, and by observational tests of theoretically predicted size distributions and waiting time distributions. Attempts have been undertaken to import physical models into the numerical SOC toy models, such as the discretization of magneto-hydrodynamics (MHD) processes. The novel applications stimulated also vigorous debates about the discrimination between SOC models, SOC-like, and non-SOC processes, such as phase transitions, turbulence, random-walk diffusion, percolation, branching processes, network theory, chaos theory, fractality, multi-scale, and other complexity phenomena. We review SOC studies from the last 25 years and highlight new trends, open questions, and future challenges, as discussed during two recent ISSI workshops on this theme.
C1 [Aschwanden, Markus J.] Lockheed Martin, Solar & Astrophys Lab LMSAL, Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Crosby, Norma B.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Dimitropoulou, Michaila] Kapodistrian Univ Athens, Dept Phys, Athens 15483, Greece.
[Georgoulis, Manolis K.] Acad Athens, Res Ctr Astron & Appl Math, Athens 11527, Greece.
[Hergarten, Stefan] Univ Freiburg, Inst Geo & Umweltnat Wissensch, D-79104 Freiburg, Germany.
[McAteer, James] New Mexico State Univ, Dept Astron, Las Cruces, NM USA.
[Milovanov, Alexander V.] Ctr Ric Frascati, ENEA Natl Lab, I-00044 Rome, Italy.
[Milovanov, Alexander V.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Milovanov, Alexander V.] Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany.
[Mineshige, Shin] Kyoto Univ, Dept Astron, Kyoto 6068602, Japan.
[Morales, Laura] Canadian Space Agcy, Space Sci & Technol Branch, St Hubert, PQ J3Y 8Y9, Canada.
[Nishizuka, Naoto] Natl Inst Informat & Commun Technol, Tokyo 1848795, Japan.
[Pruessner, Gunnar] Univ London Imperial Coll Sci Technol & Med, Dept Math, London SW7 2AZ, England.
[Sanchez, Raul] Univ Carlos III Madrid, Dept Fis, Madrid 28911, Spain.
[Sharma, A. Surja] Univ Maryland, Dept Astron, College Pk, MD 20740 USA.
[Strugarek, Antoine] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Uritsky, Vadim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aschwanden, MJ (reprint author), Lockheed Martin, Solar & Astrophys Lab LMSAL, Adv Technol Ctr, A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA.
EM aschwanden@lmsal.com
FU NASA of the SDO/AIA instrument [NNG04EA00C]; EU [PIRG07-GA-2010-268245];
NASA [NNX11A099G]
FX The author team acknowledges the hospitality and partial support for two
workshops on "Self-Organized Criticality and Turbulence" at the
International Space Science Institute (ISSI) at Bern, Switzerland,
during October 15-19, 2012, and September 16-20, 2013, as well as
constructive and stimulating discussions (in alphabetical order) with
Sandra Chapman, Paul Charbonneau, Henrik Jeldtoft Jensen, Maya Paczuski,
Jens Juul Rasmussen, John Rundle, Loukas Vlahos, and Nick Watkins. This
work was partially supported by NASA contract NNX11A099G "Self-organized
criticality in solar physics" and NASA contract NNG04EA00C of the
SDO/AIA instrument to LMSAL. MKG acknowledges partial support by the EU
Seventh Framework Marie-Curie Programme under grant agreement No.
PIRG07-GA-2010-268245.
NR 564
TC 16
Z9 17
U1 12
U2 31
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JAN
PY 2016
VL 198
IS 1-4
BP 47
EP 166
DI 10.1007/s11214-014-0054-6
PG 120
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ1AF
UT WOS:000366837400004
ER
PT J
AU Sharma, AS
Aschwanden, MJ
Crosby, NB
Klimas, AJ
Milovanov, AV
Morales, L
Sanchez, R
Uritsky, V
AF Sharma, A. Surjalal
Aschwanden, Markus J.
Crosby, Norma B.
Klimas, Alexander J.
Milovanov, Alexander V.
Morales, Laura
Sanchez, Raul
Uritsky, Vadim
TI 25 Years of Self-organized Criticality: Space and Laboratory Plasmas
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Self-organized criticality; Nonequilibrium systems; Multiscale
phenomena; Turbulence; Space plasmas; Tokamaks
ID LONG-RANGE CORRELATIONS; DETRENDED FLUCTUATION ANALYSIS;
MAGNETOSPHERE-IONOSPHERE SYSTEM; MAGNETIC CONFINEMENT DEVICES;
MAGNETOTAIL CURRENT SHEET; AURORAL ELECTROJET INDEX; SOLAR-WIND
FLUCTUATIONS; SIMPLE AVALANCHE MODEL; POWER-LAW DISTRIBUTION; DUAL
SCALING REGIMES
AB Studies of complexity in extended dissipative dynamical systems, in nature and in laboratory, require multiple approaches and the framework of self-organized criticality (SOC) has been used extensively in the studies of such nonequilibrium systems. Plasmas are inherently nonlinear and many ubiquitous features such as multiscale behavior, intermittency and turbulence have been analyzed using SOC concepts. The role of SOC in advancing our understanding of space and laboratory plasmas as nonequilibrium systems is reviewed in this article. The main emphasis is on how SOC and related approaches have provided new insights and models of nonequilibrium plasma phenomena. Among the natural plasmas the magnetosphere, driven by the solar wind, is a prominent example and extensive data from ground-based and space-borne instruments have been used to study phenomena of direct relevance to space weather, viz. geomagnetic storms and substorms. During geomagnetically active periods the magnetosphere is far from equilibrium, due to its internal dynamics and being driven by the turbulent solar wind, and substorms are prominent features of the complex driven system. Studies using solar wind and magnetospheric data have shown both global and multiscale features of substorms. While the global behavior exhibits system-wide changes, the multiscale behavior shows scaling features. Along with the studies based on observational data, analogue models of the magnetosphere have advanced the understanding of space plasmas as well as the role of SOC in natural systems. In laboratory systems, SOC has been used in modeling the plasma behavior in fusion experiments, mainly in tokamaks and stellarators. Tokamaks are the dominant plasma confinement system and modeling based on SOC have provided a complementary approach to the understanding of plasma behavior under fusion conditions. These studies have provided insights into key features of toroidally confined plasmas, e.g., the existence of critical temperature gradients above which the transport rates increase drastically. The SOC models address the transport properties from a more general approach, compared to those based on turbulence arising from specific plasma instabilities, and provide a better framework for modeling features such as superdiffusion. The studies of space and laboratory plasmas as nonequilibrium systems have been motivated by features such as scaling and critical behavior, and have provided new insights by highlighting the properties that are common with other systems.
C1 [Sharma, A. Surjalal] Univ Maryland, Dept Astron, College Pk, MD 20740 USA.
[Aschwanden, Markus J.] Lockheed Martin, Solar & Astrophys Lab LMSAL, Palo Alto, CA 94304 USA.
[Crosby, Norma B.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Klimas, Alexander J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Milovanov, Alexander V.] Ctr Ric Frascati, ENEA Natl Lab, I-00044 Rome, Italy.
[Milovanov, Alexander V.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Morales, Laura] Canadian Space Agcy, Space Sci & Technol Branch, St Hubert, PQ J3Y 8Y9, Canada.
[Sanchez, Raul] Univ Carlos III Madrid, Dept Fis, Madrid 28911, Spain.
[Uritsky, Vadim] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sharma, AS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20740 USA.
EM ssh@astro.umd.edu
FU NSF [AGS-1036473, IIP-1338634]
FX The author team acknowledges the hospitality and partial support for two
workshops on "Self-Organized Criticality and Turbulence" at the
International Space Science Institute (ISSI) in Bern, Switzerland,
during October 15-19, 2012, and September 16-20, 2013. Discussions with
V.P. Budaev, J. Chen, G. Dif-Pradalier, A. Iomin, P.K. Kaw, V.
Krishnamurthy, K. Papadopoulos, J.J. Rasmussen, A. Sen, X. Shao, M.I.
Sitnov, A.Y. Ukhorskiy, D. Vassiliadis, T. Veeramani, L.M. Zelenyi, and
F. Zonca are gratefully acknowledged. The research at the University of
Maryland was supported by NSF grants AGS-1036473 and IIP-1338634.
NR 332
TC 4
Z9 4
U1 8
U2 25
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JAN
PY 2016
VL 198
IS 1-4
BP 167
EP 216
DI 10.1007/s11214-015-0225-0
PG 50
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ1AF
UT WOS:000366837400005
ER
PT J
AU McAteer, RTJ
Aschwanden, MJ
Dimitropoulou, M
Georgoulis, MK
Pruessner, G
Morales, L
Ireland, J
Abramenko, V
AF McAteer, R. T. James
Aschwanden, Markus J.
Dimitropoulou, Michaila
Georgoulis, Manolis K.
Pruessner, Gunnar
Morales, Laura
Ireland, Jack
Abramenko, Valentyna
TI 25 Years of Self-organized Criticality: Numerical Detection Methods
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Self organized criticality; Numerical methods
ID SEQUENTIAL CHROMOSPHERIC BRIGHTENINGS; WAITING-TIME DISTRIBUTION; SOLAR
MAGNETIC TRACKING; POLAR CORONAL HOLE; ACTIVE REGIONS; QUIET-SUN;
SPATIOTEMPORAL EVOLUTION; ENERGY-DISTRIBUTION; MULTIWAVELENGTH
OBSERVATIONS; STATISTICAL-ANALYSIS
AB The detection and characterization of self-organized criticality (SOC), in both real and simulated data, has undergone many significant revisions over the past 25 years. The explosive advances in the many numerical methods available for detecting, discriminating, and ultimately testing, SOC have played a critical role in developing our understanding of how systems experience and exhibit SOC. In this article, methods of detecting SOC are reviewed; from correlations to complexity to critical quantities. A description of the basic autocorrelation method leads into a detailed analysis of application-oriented methods developed in the last 25 years. In the second half of this manuscript space-based, time-based and spatial-temporal methods are reviewed and the prevalence of power laws in nature is described, with an emphasis on event detection and characterization. The search for numerical methods to clearly and unambiguously detect SOC in data often leads us outside the comfort zone of our own disciplines-the answers to these questions are often obtained by studying the advances made in other fields of study. In addition, numerical detection methods often provide the optimum link between simulations and experiments in scientific research. We seek to explore this boundary where the rubber meets the road, to review this expanding field of research of numerical detection of SOC systems over the past 25 years, and to iterate forwards so as to provide some foresight and guidance into developing breakthroughs in this subject over the next quarter of a century.
C1 [McAteer, R. T. James] New Mexico State Univ, Dept Astron, Solar Phys & Space Weather, Las Cruces, NM 88003 USA.
[Aschwanden, Markus J.] STAR Labs, LMSAL, Palo Alto, CA 94304 USA.
[Dimitropoulou, Michaila] Kapodistrian Univ Athens, Dept Phys, Athens 15483, Greece.
[Georgoulis, Manolis K.] Acad Athens, Astron & Appl Math Res Ctr, Athens 11527, Greece.
[Pruessner, Gunnar] Univ London Imperial Coll Sci Technol & Med, Dept Math, London SW7 2AZ, England.
[Morales, Laura] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Fis, Inst Fis Plasmas CONICET, RA-1428 Buenos Aires, DF, Argentina.
[Ireland, Jack] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
[Abramenko, Valentyna] Russian Acad Sci Pulkovo, Dept Solar Phys, Cent Astron Observ, Space Weather Predict Lab, St Petersburg 196140, Russia.
[Abramenko, Valentyna] NJIT, Big Bear Solar Observ, Big Bear City, CA 92314 USA.
RP McAteer, RTJ (reprint author), New Mexico State Univ, Dept Astron, Solar Phys & Space Weather, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.
EM mcateer@nmsu.edu
FU National Science Foundation [AGS-1255024]; NASA [NNH12CG10C, NNX13AE03G,
NNX11A099G]; NASA of the SDO/AIA instrument [NG04EA00C]; EU
[PIRG07-GA-2010-268245]; NASA LWS [NNX11AO73G]; Program of the Presidium
of Russian Academy of Sciences [21]
FX The author team acknowledges the hospitality and partial support for two
workshops on Self-Organized Criticality and Turbulence at the
International Space Science Institute (ISSI) at Bern, Switzerland,
during October 15-19, 2012, and September 16-20, 2013. One of us (JMA)
was partially supported by a National Science Foundation Career award,
NSF AGS-1255024, and NASA contracts NNH12CG10C and NNX13AE03G. One of us
(MJA) was partially supported by NASA contract NNX11A099G and NASA
contract NG04EA00C of the SDO/AIA instrument to LMSAL. One of us (MKG)
was partially supported by EU FP7 grant PIRG07-GA-2010-268245. One of us
(VIA) was partially supported by NASA LWS NNX11AO73G grant and by the
Program of the Presidium of Russian Academy of Sciences No. 21. The
authors acknowledge the comprehensive and dedicated work of an anonymous
referee.
NR 148
TC 3
Z9 3
U1 3
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JAN
PY 2016
VL 198
IS 1-4
BP 217
EP 266
DI 10.1007/s11214-015-0158-7
PG 50
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ1AF
UT WOS:000366837400006
ER
PT J
AU Konings, AG
Piles, M
Rotzer, K
McColl, KA
Chan, SK
Entekhabi, D
AF Konings, Alexandra G.
Piles, Maria
Roetzer, Kathrina
McColl, Kaighin A.
Chan, Steven K.
Entekhabi, Dara
TI Vegetation optical depth and scattering albedo retrieval using time
series of dual-polarized L-band radiometer observations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Vegetation optical depth; Single-scattering albedo; Soil dielectric
constant; Soil moisture; Vegetation water content; L-band radiometry;
Aquarius/SAC-D; SMAP
ID SOIL-MOISTURE RETRIEVAL; MICROWAVE EMISSION; SATELLITE-OBSERVATIONS;
DIFFERENCE INDEX; SMOS; MODEL; ALGORITHM; AQUARIUS; WATER; SENSITIVITY
AB Passive microwave measurements have the potential to estimate vegetation optical depth (VOD), an indicator of aboveground vegetation water content. They are also sensitive to the vegetation scattering albedo and soil moisture. In this work, we propose a novel algorithm to retrieve VOD and soil moisture from time series of dual-polarized L-band radiometric observations along with time-invariant scattering albedo. The method takes advantage of the relatively slow temporal dynamics of early morning vegetation water content and combines a number of consecutive observations to estimate a single VOD. It is termed the multi-temporal dual channel algorithm (MT-DCA). The soil dielectric constant (directly related to soil moisture) of each observation is also retrieved simultaneously. Additionally, the method retrieves a constant albedo, thereby providing for the first time information on global single-scattering albedo variations. The algorithm is tested using three years of L-band passive observations from the NASA Aquarius sensor. The global VOD distribution follows expected gradients of climate and canopy biomass conditions. Its seasonal dynamics follow expected behavior based on precipitation and land cover. The retrieved VOD is closely related to coincident cross-polarized backscatter coefficients. The VOD and dielectric retrievals from MT-DCA are compared to those obtained from implementing the commonly used Land Parameter Retrieval Model (LPRM) algorithm and shown to have less high-frequency noise. There is almost as much variation in MT-DCA retrieved albedo between pixels of a given land cover class than between land cover classes, suggesting the common approach of assigning albedo based on land cover class may not capture its spatial variability. Globally, albedo appears to be primarily sensitive to woody biomass. The proposed algorithm allows for a more accurate accounting of the effects of vegetation on radiometric soil moisture retrievals, and generates new observations of L-band VOD and effective single-scattering albedo. These new datasets are complementary to existing remotely sensed vegetation measurements such as fluorescence and optical-infrared indices. (C) 2015 Elsevier Inc All rights reserved.
C1 [Konings, Alexandra G.; McColl, Kaighin A.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA.
[Piles, Maria] UPC, Dept Teoria Senyal & Comunicac, IEEC UPC, Barcelona 08034, Spain.
[Piles, Maria] SMOS BEC, Barcelona 08034, Spain.
[Roetzer, Kathrina] Forschungszentrum Julich, Agrosphere Inst, D-52428 Julich, Germany.
[Chan, Steven K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Konings, AG (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
OI Piles, Maria/0000-0002-1169-3098; Konings, Alexandra/0000-0002-2810-1722
FU NASA Soil Moisture Active Passive project; MIT International Science and
Technology Initiatives (MISTI); Spanish Ministry of Science and
Education [AYA2012-39356-C05-01]; BBVA Foundation; NASA Earth and Space
Science Fellowship Program; NSF Graduate Research Fellowship
FX The authors acknowledge the support of the NASA Soil Moisture Active
Passive project for this study. Partial funding was also received from
the MIT International Science and Technology Initiatives (MISTI), the
Spanish Ministry of Science and Education under the project
AYA2012-39356-C05-01, the BBVA Foundation, and the NASA Earth and Space
Science Fellowship Program (A.G.K.) and NSF Graduate Research Fellowship
(K.A.M.). The data are available from the authors upon request.
NR 57
TC 7
Z9 7
U1 10
U2 22
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN
PY 2016
VL 172
BP 178
EP 189
DI 10.1016/j.rse.2015.11.009
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CY9ZI
UT WOS:000366764500014
ER
PT J
AU Ferguson, JC
Panerai, F
Lachaud, J
Martin, A
Bailey, SCC
Mansour, NN
AF Ferguson, Joseph C.
Panerai, Francesco
Lachaud, Jean
Martin, Alexandre
Bailey, Sean C. C.
Mansour, Nagi N.
TI Modeling the oxidation of low-density carbon fiber material based on
micro-tomography
SO CARBON
LA English
DT Article
DE Carbon fibre; Oxidation; Micro-tomography
ID C/C COMPOSITE; ABLATION
AB Oxidation is one of the main decomposition mechanisms of fibrous carbon/phenolic ablators employed in thermal protection systems for planetary entry capsules. The oxidation process is driven by two competing mechanisms: diffusion of reactants within the porous medium, and reaction rates at the surface of the fibers. These mechanisms are characterized by the Thiele number. Given that the Thiele number varies during an atmospheric entry, we aim to understand the effects of the diffusion/reaction processes on the decomposition of a porous carbon material in various regimes. We use a particle method for simulations of the oxidation process at microscale. The movement of oxygen reactants is simulated using a Brownian motion technique, and heterogeneous first-order reactions at the surface are modeled with a sticking probability law. To enable simulations of the fiber decomposition on actual materials, we use digitized computational grids obtained using X-ray micro-tomographic imaging. We present results for the oxidation of the substrate of the material used on the Mars Science laboratory capsule that landed the Curiosity rover. We find that the depth of the reaction zone for this material is critically dependent on the Thiele number. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Ferguson, Joseph C.; Panerai, Francesco; Martin, Alexandre; Bailey, Sean C. C.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Lachaud, Jean] Univ Calif Santa Cruz, Silicon Valley Initiat, Moffett Field, CA 94035 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
RP Panerai, F (reprint author), Univ Kentucky, Dept Mech Engn, 151 Ralph G Anderson Bldg, Lexington, KY 40506 USA.
EM francesco.panerai@uky.edu
OI Martin, Alexandre/0000-0003-2216-2468; Lachaud, Jean/0000-0001-7397-1025
FU NASA SBIR Phase II Award [NNX10CC53P]; NASA; Kentucky EPSCoR Award
[NNX13AN04A, NNX14AI97G]; NASA Kentucky under NASA [NNX10AL96H]; Office
of Science, Office of Basic Energy Sciences, of the U.S. Department of
Energy [DE-AC02-05CH11231]
FX The authors are indebted to T.A. Sandstrom for his assistance in the
development of the PUMA framework. A.A. McDowell and D.Y. Parkinson are
gratefully acknowledged for their help in the LBNL/NASA Ames
collaboration on micro-CT measurements. This work was performed under
the Entry System Modeling Project (M.J. Wright project manager) of the
NASA Game Changing Development (GCD) Program. The work was partly
supported by NASA SBIR Phase II Award NNX10CC53P, NASA and Kentucky
EPSCoR Award NNX13AN04A, NASA Award NNX14AI97G, and NASA Kentucky under
NASA Award NNX10AL96H. The Advanced Light Source is supported by the
Director, Office of Science, Office of Basic Energy Sciences, of the
U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
NR 19
TC 2
Z9 2
U1 4
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0008-6223
EI 1873-3891
J9 CARBON
JI Carbon
PD JAN
PY 2016
VL 96
BP 57
EP 65
DI 10.1016/j.carbon.2015.08.113
PG 9
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA CY0EB
UT WOS:000366078000008
ER
PT J
AU Islam, T
Srivastava, PK
Petropoulos, GP
Singh, SK
AF Islam, Tanvir
Srivastava, Prashant K.
Petropoulos, George P.
Singh, Sudhir K.
TI Reduced major axis approach for correcting GPM/GMI radiometric biases to
coincide with radiative transfer simulation
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Bias correction and estimation; Radiometric adjustment; Radiative
transfer model; Radiance assimilation; Satellite calibration; Global
Precipitation Measurement (GPM)
ID DATA ASSIMILATION; CORRECTION SCHEME; SYSTEM; MODEL; PERFORMANCE;
VALIDATION; ALGORITHM; CODE
AB Correcting radiometric biases is crucial prior to the use of satellite observations in a physically based retrieval or data assimilation system. This study proposes an algorithm - RARMA (Radiometric Adjustment using Reduced Major Axis) for correcting the radiometric biases so that the observed radiances coincide with the simulation of a radiative transfer model. The RARMA algorithm is a static bias correction algorithm, which is developed using the reduced major axis (RMA) regression approach. NOAA's Community Radiative Transfer Model (CRTM) has been used as the basis of radiative transfer simulation for adjusting the observed radiometric biases. The algorithm is experimented and applied to the recently launched Global Precipitation Measurement (GPM) mission's GPM Microwave Imager (GMI). Experimental results demonstrate that radiometric biases are apparent in the GMI instrument. The RARMA algorithm has been able to correct such radiometric biases and a significant reduction of observation residuals is revealed while assessing the performance of the algorithm. The experiment is currently tested on clear scenes and over the ocean surface, where, surface emissivity is relatively easier to model, with the help of a microwave emissivity model (FASTEM-5). (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Islam, Tanvir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Islam, Tanvir] NOAA NESDIS STAR, College Pk, MD USA.
[Srivastava, Prashant K.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3FG, Dyfed, Wales.
[Singh, Sudhir K.] Univ Allahabad, Ctr Atmospher & Ocean Studies, Allahabad 211002, Uttar Pradesh, India.
RP Islam, T (reprint author), CALTECH, Jet Prop Lab, Earth Sci Sect 329B, M-S 183-518 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tanvir.islam@jpl.nasa.gov
RI Petropoulos, George/F-2384-2013
OI Petropoulos, George/0000-0003-1442-1423
NR 27
TC 1
Z9 1
U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2016
VL 168
BP 40
EP 45
DI 10.1016/j.jqsrt.2015.08.016
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CX9EE
UT WOS:000366007000005
ER
PT J
AU Berdyugina, SV
Kuhn, JR
Harrington, DM
Santl-Temkiv, T
Messersmith, EJ
AF Berdyugina, Svetlana V.
Kuhn, Jeff R.
Harrington, David M.
Santl-Temkiv, Tina
Messersmith, E. John
TI Remote sensing of life: polarimetric signatures of photosynthetic
pigments as sensitive biomarkers
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE biopigments; biosignatures; Earth-like planets; exoplanets;
photosynthesis; remote sensing of life; spectropolarimetry
ID SPECTRAL SIGNATURES; EXTRASOLAR PLANETS; EARTH; POLARIZATION;
REFLECTANCE; LIGHT; BIOSIGNATURES; ATMOSPHERE; LEAVES; SUN
AB We develop a polarimetry-based remote-sensing method for detecting and identifying life forms in distant worlds and distinguishing them from non-biological species. To achieve this we have designed and built a bio-polarimetric laboratory experiment BioPol for measuring optical polarized spectra of various biological and non-biological samples. Here we focus on biological pigments, which are common in plants and bacteria that employ them either for photosynthesis or for protection against reactive oxygen species. Photosynthesis, which provides organisms with the ability to use light as a source of energy, emerged early in the evolution of life on Earth. The ability to harvest such a significant energy resource could likely also develop on habited exoplanets. Thus, we investigate the detectability of biomolecules that can capture photons of particular wavelengths and contribute to storing their energy in chemical bonds. We have carried out laboratory spectropolarimetric measurements of a representative sample of plants containing various amounts of pigments such as chlorophyll, carotenoids and others. We have also measured a variety of non-biological samples (sands, rocks). Using our lab measurements, we have modelled intensity and polarized spectra of Earth-like planets having different surface coverage by photosynthetic organisms, deserted land and ocean, as well as clouds. Our results demonstrate that linearly polarized spectra provide very sensitive and rather unambiguous detection of photosynthetic pigments of various kinds. Our work paves the path towards analogous measurements of microorganisms and remote sensing of microbial ecology on the Earth and of extraterrestrial life on other planets and moons.
C1 [Berdyugina, Svetlana V.; Harrington, David M.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Berdyugina, Svetlana V.] Univ Hawaii, NASA, Inst Astron, Astrobiol Inst, Honolulu, HI 96822 USA.
[Kuhn, Jeff R.; Harrington, David M.; Messersmith, E. John] Univ Hawaii, Inst Astron, Maui, HI 96768 USA.
[Santl-Temkiv, Tina] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Aarhus, Denmark.
RP Berdyugina, SV (reprint author), Kiepenheuer Inst Sonnenphys, Schoneckstr 6, D-79104 Freiburg, Germany.
EM sveta@kis.uni-freiburg.de
FU Leibniz Association, Germany [SAW-2011-KIS-7]; European Research Council
[291659, 267864]; Danish National Research Foundation [DNRF106]; NASA
Astrobiology Institute; Institute for Astronomy, University of Hawaii,
USA
FX This work was supported by the SAW-2011-KIS-7 grant provided by the
Leibniz Association, Germany, and the Advance Grant projects HotMol and
ASTERISK provided by the European Research Council (grant agreements
291659 and 267864, respectively). Funding for the Stellar Astrophysics
Centre is provided by The Danish National Research Foundation (Grant
agreement no.: DNRF106). SB acknowledges support by the NASA
Astrobiology Institute and Institute for Astronomy, University of
Hawaii, USA. We thank anonymous referees for thorough reviews which
helped to improve the manuscript.
NR 35
TC 3
Z9 3
U1 5
U2 32
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
EI 1475-3006
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD JAN
PY 2016
VL 15
IS 1
BP 45
EP 56
DI 10.1017/S1473550415000129
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CX6PW
UT WOS:000365824000008
ER
PT J
AU Verseux, C
Baque, M
Lehto, K
de Vera, JPP
Rothschild, LJ
Billi, D
AF Verseux, Cyprien
Baque, Mickael
Lehto, Kirsi
de Vera, Jean-Pierre P.
Rothschild, Lynn J.
Billi, Daniela
TI Sustainable life support on Mars - the potential roles of cyanobacteria
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE cyanobacteria; in situ resource utilization (ISRU); life-support
systems; Mars exploration; space technologies; synthetic biology
ID NITROGEN-FIXING CYANOBACTERIUM; IONIZING-RADIATION RESISTANCE; DURATION
EXPLORATORY MISSIONS; MICROBE-MINERAL INTERACTIONS; BLUE-GREEN-ALGAE;
LOW-EARTH-ORBIT; SP PCC 6803; ESCHERICHIA-COLI; SYNTHETIC BIOLOGY;
BACILLUS-SUBTILIS
AB Even though technological advances could allow humans to reach Mars in the coming decades, launch costs prohibit the establishment of permanent manned outposts for which most consumables would be sent from Earth. This issue can be addressed by in situ resource utilization: producing part or all of these consumables on Mars, from local resources. Biological components are needed, among other reasons because various resources could be efficiently produced only by the use of biological systems. But most plants and microorganisms are unable to exploit Martian resources, and sending substrates from Earth to support their metabolism would strongly limit the cost-effectiveness and sustainability of their cultivation. However, resources needed to grow specific cyanobacteria are available on Mars due to their photosynthetic abilities, nitrogen-fixing activities and lithotrophic lifestyles. They could be used directly for various applications, including the production of food, fuel and oxygen, but also indirectly: products from their culture could support the growth of other organisms, opening the way to a wide range of life-support biological processes based on Martian resources. Here we give insights into how and why cyanobacteria could play a role in the development of self-sustainable manned outposts on Mars.
C1 [Verseux, Cyprien; Baque, Mickael; Billi, Daniela] Univ Roma Tor Vergata, Dept Biol, I-00173 Rome, Italy.
[Verseux, Cyprien] NASA, Ames Res Ctr, NASA EAP Associate, Moffett Field, CA 94035 USA.
[Lehto, Kirsi] Univ Turku, Dept Plant Physiol & Mol Biol, Turku, Finland.
[Lehto, Kirsi] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[de Vera, Jean-Pierre P.] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA.
RP Verseux, C (reprint author), Univ Roma Tor Vergata, Dept Biol, I-00173 Rome, Italy.
EM cyprien.verseux@gmail.com
FU Italian Space Agency
FX The authors are grateful to Sean McMahon (Yale University) for his
remarkable artistic rendering. They thank Rocco L. Mancinelli and an
anonymous reviewer, whose comments led to significant improvements to
the manuscript. They are also grateful to Ivan G. Paulino-Lima, Kosuke
Fujishima, Ryan Kent, Griffin McCutcheon, Evie Pless, Jesica Navarrete,
Diana Gentry and J. Mike Grace (Lynn Rothschild's laboratory, NASA Ames
Research Center) for stimulating discussions. Finally, they thank
Christiane Heinicke (Aalto University) for proofreading the penultimate
version of the manuscript. This work was supported by the Italian Space
Agency, noteworthy through their support to the BIOMEX_Cyano and
BOSS_Cyano experiments. It was also supported by CV's appointment to the
NASA Education Associates Program managed by the Universities Space
Research Association.
NR 284
TC 4
Z9 4
U1 43
U2 130
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
EI 1475-3006
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD JAN
PY 2016
VL 15
IS 1
BP 65
EP 92
DI 10.1017/S147355041500021X
PG 28
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CX6PW
UT WOS:000365824000010
ER
PT J
AU Walsh, BM
Lee, HR
Barnes, NP
AF Walsh, Brian M.
Lee, Hyung R.
Barnes, Norman P.
TI Mid infrared lasers for remote sensing applications
SO JOURNAL OF LUMINESCENCE
LA English
DT Article; Proceedings Paper
CT 17th International Conference on Luminescence and Optical Spectroscopy
of Condensed Matter (ICL)
CY JUL 13-18, 2014
CL Univ Wroclaw, Fac Law, Adm & Econ, Wroclaw, POLAND
SP Polish Acad Sci, Inst Low Temp & Struct Res, Univ Wroclaw, Fac Chem, Wroclaw Univ Econ, Fundacja Uniwersytetu Wroclawskiego
HO Univ Wroclaw, Fac Law, Adm & Econ
DE Lanthanide-doped materials; Low phonon materials; Mid-infrared lasers;
Atmospheric remote sensing
ID CRYSTALS
AB To accurately measure the concentrations of atmospheric gasses, especially the gasses with low concentrations, strong absorption features must be accessed. Each molecular species or constituent has characteristic mid-infrared absorption features by which either column content or range resolved concentrations can be measured. Because of these characteristic absorption features the mid infrared spectral region is known as the fingerprint region. However, as noted by the Decadal Survey, mid-infrared solid-state lasers needed for DIAL systems are not available. The primary reason is associated with short upper laser level lifetimes of mid infrared transitions. Energy gaps between the energy levels that produce mid-infrared laser transitions are small, promoting rapid nonradiative quenching. Non-radiative quenching is a multiphonon process, the more phonons needed, the smaller the effect. More low energy phonons are required to span an energy gap than high energy phonons. Thus, low energy phonon materials have less nonradiative quenching compared to high energy phonon materials. Common laser materials, such as oxides like YAG, are high phonon energy materials, while fluorides, chlorides and bromides are low phonon materials. Work at NASA Langley is focused on a systematic search for novel lanthanide-doped mid-infrared solid-state lasers using both quantum mechanical models (theoretical) and spectroscopy (experimental) techniques. Only the best candidates are chosen for laser studies. The capabilities of modeling materials, experimental challenges, material properties, spectroscopy, and prospects for lanthanide-doped mid-infrared solid-state laser devices will be presented. Published by Elsevier B.V.
C1 [Walsh, Brian M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Lee, Hyung R.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Barnes, Norman P.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Walsh, BM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM brian.m.walsh@nasa.gov
NR 7
TC 5
Z9 5
U1 3
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-2313
EI 1872-7883
J9 J LUMIN
JI J. Lumines.
PD JAN
PY 2016
VL 169
BP 400
EP 405
DI 10.1016/j.jlumin.2015.03.004
PN B
PG 6
WC Optics
SC Optics
GA CX3NQ
UT WOS:000365606200006
ER
PT J
AU Strekalov, DV
Kowligy, AS
Velev, VG
Kanter, GS
Kumar, P
Huang, YP
AF Strekalov, Dmitry V.
Kowligy, Abijith S.
Velev, Vesselin G.
Kanter, Gregory S.
Kumar, Prem
Huang, Yu-Ping
TI Phase matching for the optical frequency conversion processes in
whispering gallery mode resonators
SO JOURNAL OF MODERN OPTICS
LA English
DT Article; Proceedings Paper
CT 45th Winter Colloquium on the Physics of Quantum Electronic
CY JAN 04-08, 2015
CL Snowbird, UT
SP Marlan Scully Texas A&M Univ, Princeton Univ, George R Welch Texas A&M Univ
DE whispering gallery modes; phase matching; nonlinear optical conversion;
quantum optics
ID BETA-BARIUM-BORATE; DISPERSION
AB Optical nonlinear processes in whispering gallery mode resonators require the phase matching that is profoundly different from that in bulk crystals or waveguides. We analyze the phase matching conditions for frequency doubling and parametric down conversion in the resonators, and find the configurations allowing for simultaneous occurrence of these two processes. Such double phase matching gives us access to a variety of interesting quantum nonlinear optical phenomena. For example, it can lead to antibunched emission of photon pairs through the quantum Zeno photonic blockade.
C1 [Strekalov, Dmitry V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Kowligy, Abijith S.; Velev, Vesselin G.; Kanter, Gregory S.; Kumar, Prem] Northwestern Univ, Ctr Photon Commun & Comp, Evanston, IL USA.
[Huang, Yu-Ping] Stevens Inst Technol, Dept Phys & Engn Phys, Hoboken, NJ 07030 USA.
RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM dmitry.v.strekalov@jpl.nasa.gov
RI Kumar, Prem/B-6691-2009
FU DARPA [W31P4Q-13-1-0004]; National Aeronautics and Space Administration
FX The research described in this paper was supported by the DARPA Quiness
program [grant number # W31P4Q-13-1-0004] carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration, and by
the Northwestern University.
NR 37
TC 1
Z9 1
U1 1
U2 11
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0950-0340
EI 1362-3044
J9 J MOD OPTIC
JI J. Mod. Opt.
PY 2016
VL 63
IS 1
SI SI
BP 50
EP 63
DI 10.1080/09500340.2015.1063726
PG 14
WC Optics
SC Optics
GA CX7QK
UT WOS:000365896900009
ER
PT J
AU Mathias, DL
Mattenberger, CJ
Go, S
AF Mathias, Donovan L.
Mattenberger, Christopher J.
Go, Susie
TI Engineering Risk Assessment of a dynamic space propulsion system
benchmark problem
SO RELIABILITY ENGINEERING & SYSTEM SAFETY
LA English
DT Article; Proceedings Paper
CT 12th International Association for Probabilistic Safety
AssessmentandManagement(PSAM12)Conference
CY JUN 22-27, 2014
CL Honolulu, HI
DE PRA; RISK simulation; Dynamic PSA; PSAM space propulsion system
benchmark problem
AB The Engineering Risk Assessment (ERA) team at NASA Ames Research Center develops dynamic models with linked physics-of-failure analyses to produce quantitative risk assessments of space exploration missions. This paper applies the ERA approach to the 2014 Probabilistic Safety Assessment and Management conference Space Propulsion System Benchmark Problem, which investigates dynamic system risk for a deep space ion propulsion system over three missions with time-varying thruster requirements and operations schedules. The dynamic missions are simulated using commercial software to generate integrated loss-of-mission (LOM) probability results via Monte Carlo sampling. The simulation model successfully captured all dynamics aspects of the benchmark missions, and convergence studies are presented to illustrate the sensitivity of integrated LOM results to the number of Monte Carlo trials. In addition, to evaluate the relative importance of dynamic modeling, the Ames Reliability Tool (ART) was used to build a series of quasi-dynamic, deterministic models that incorporated varying levels of the problem's dynamics. The ART model did a reasonable job of matching the simulation results for the simpler mission case, while auxiliary dynamic models were required to adequately capture risk-driver rankings for the more dynamic cases. This study highlights how state-of-the-art techniques can adapt to a range of dynamic problems. Published by Elsevier Ltd.
C1 [Mathias, Donovan L.; Go, Susie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Mattenberger, Christopher J.] Sci & Technol Corp, NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Mathias, DL (reprint author), NASA, Ames Res Ctr, MS 258-5, Moffett Field, CA 94035 USA.
EM Donovan.Mathias@nasa.gov; christopher.j.mattenberger@nasa.gov;
susie.go@nasa.gov
NR 15
TC 0
Z9 0
U1 2
U2 14
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0951-8320
EI 1879-0836
J9 RELIAB ENG SYST SAFE
JI Reliab. Eng. Syst. Saf.
PD JAN
PY 2016
VL 145
BP 316
EP 328
DI 10.1016/j.ress.2015.07.003
PG 13
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA CX0DO
UT WOS:000365367300031
ER
PT J
AU Benjamin, A
Dezfuli, H
Everett, C
AF Benjamin, Allan
Dezfuli, Homayoon
Everett, Chris
TI Developing probabilistic safety performance margins for unknown and
underappreciated risks
SO RELIABILITY ENGINEERING & SYSTEM SAFETY
LA English
DT Article; Proceedings Paper
CT 12th International Association for Probabilistic Safety
AssessmentandManagement(PSAM12)Conference
CY JUN 22-27, 2014
CL Honolulu, HI
DE Probabilistic; Safety performance margin; Safety performance
requirement; Safety threshold; Safety goal; Unknown risk;
Underappreciated risk
AB Probabilistic safety requirements currently formulated or proposed for space systems, nuclear reactor systems, nuclear weapon systems, and other types of systems that have a low-probability potential for high-consequence accidents depend on showing that the probability of such accidents is below a specified safety threshold or goal. Verification of compliance depends heavily upon synthetic modeling techniques such as PRA. To determine whether or not a system meets its probabilistic requirements, it is necessary to consider whether there are significant risks that are not fully considered in the PRA either because they are not known at the time or because their importance is not fully understood. The ultimate objective is to establish a reasonable margin to account for the difference between known risks and actual risks in attempting to validate compliance with a probabilistic safety threshold or goal. In this paper, we examine data accumulated over the past 60 years primarily from the space program, and secondarily from nuclear reactor experience, aircraft systems, and human reliability experience to formulate guidelines for estimating probabilistic margins to account for risks that are initially unknown or underappreciated. The formulation includes a review of the safety literature to identify the principal causes of such risks. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Dezfuli, Homayoon] NASA Headquarters, Off Safety & Mission Assurance, Washington, DC USA.
[Everett, Chris] Informat Syst Labs Inc, Rockville, MD USA.
EM asbenja@q.com; hdezfuli@nasa.gov; ceverett@islinc.com
NR 34
TC 0
Z9 0
U1 3
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0951-8320
EI 1879-0836
J9 RELIAB ENG SYST SAFE
JI Reliab. Eng. Syst. Saf.
PD JAN
PY 2016
VL 145
BP 329
EP 340
DI 10.1016/j.ress.2015.07.021
PG 12
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA CX0DO
UT WOS:000365367300032
ER
PT J
AU Coughlin, DR
Casalena, L
Yang, F
Noebe, RD
Mills, MJ
AF Coughlin, D. R.
Casalena, L.
Yang, F.
Noebe, R. D.
Mills, M. J.
TI Microstructure-property relationships in a high-strength 51Ni-29Ti-20Hf
shape memory alloy
SO JOURNAL OF MATERIALS SCIENCE
LA English
DT Article
ID NICKEL-ALUMINUM SYSTEM; MARTENSITIC-TRANSFORMATION;
MECHANICAL-PROPERTIES; PRECIPITATE PHASE; BEHAVIOR; STEM
AB NiTiHf alloys exhibit remarkable shape memory and pseudoelastic properties that are of fundamental interest to a growing number of industries. In this study, differential scanning calorimetry and isothermal compression tests have revealed that the 51Ni-29Ti-20Hf alloy has useful shape memory properties that include a wide range of transformation temperatures as well as highly stable pseudoelastic behavior. These properties are governed by short-term aging conditions, which may be tailored to control transformation temperatures while giving rise to exceptionally high austenite yield strengths which aid transformation stability. The yield strength of the austenite phase can reach 2.1 GPa by aging for 3 h at 500 degrees C, while aging for 3 h at 700 degrees C produced an alloy with an austenite finish temperature (A(f)) of 146 degrees C. High-resolution scanning transmission electron microscopy has revealed a new precipitate phase, H'-phase, under the homogenized and extruded conditions and under the 500 degrees C-3-h-aged condition, but only the previously identified H-phase precipitate was observed after aging at temperatures of 600 and 700 degrees C for 3 h. Finally, dislocation analysis indicated that plastic deformation of the austenite phase occurred by < 100 > type slip, similar to that observed in binary NiTi.
C1 [Coughlin, D. R.] Los Alamos Natl Lab, Div Mat Sci & Technol, Los Alamos, NM 87545 USA.
[Casalena, L.; Yang, F.; Mills, M. J.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA.
[Noebe, R. D.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44109 USA.
RP Coughlin, DR (reprint author), Los Alamos Natl Lab, Div Mat Sci & Technol, MS G770, Los Alamos, NM 87545 USA.
EM coughlin@lanl.gov
FU US Department of Energy, Office of Basic Energy Sciences [DE-SC0001258];
NASA FAP; TAC Transformational Tools & Technologies Project;
Aeronautical Sciences Project
FX This work was supported by the US Department of Energy, Office of Basic
Energy Sciences under Grant #DE-SC0001258. R.D.N. acknowledges funding
from the NASA FAP, Aeronautical Sciences Project, and the TAC
Transformational Tools & Technologies Project, Technical Discipline
Lead, Dale Hopkins.
NR 46
TC 2
Z9 2
U1 11
U2 26
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2461
EI 1573-4803
J9 J MATER SCI
JI J. Mater. Sci.
PD JAN
PY 2016
VL 51
IS 2
BP 766
EP 778
DI 10.1007/s10853-015-9400-7
PG 13
WC Materials Science, Multidisciplinary
SC Materials Science
GA CW8QI
UT WOS:000365263900012
ER
PT J
AU Daniels, JL
Smith, GL
Priestley, KJ
Thomas, S
AF Daniels, Janet L.
Smith, G. Louis
Priestley, Kory J.
Thomas, Susan
TI Using Lunar Observations to Validate Clouds and the Earth's Radiant
Energy System Pointing Accuracy
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Alignment; Aqua; Clouds and the Earth's Radiant Energy System (CERES);
pointing accuracy; Terra; validation
ID CERES; RADIOMETERS
AB To make measurements of the Earth's radiation budget, a pair of Clouds and the Earth's Radiant Energy System (CERES) instruments, i.e., Flight Models (FM) 1 and 2, have flown on the Terra spacecraft since December 1999, and a pair, i.e., FM-3 and FM-4, have flown on the Aqua spacecraft since June 2002. To produce accurate radiation fluxes at the top of the atmosphere and at various levels within the atmosphere and at the surface, CERES data are combined with higher resolution imager data. Validation is necessary to ensure that the accuracy with which the CERES footprints are located on the Earth will be adequate to use the imager data. The Moon provides a useful target for determining the pointing accuracy of the three channels of CERES. Near full moon, the CERES instruments can be turned to look at the Moon as the host spacecraft passes near the pole. The instrument scans the Moon in a raster-like pattern for a few minutes during the orbit when the Moon is in position. A technique has been developed by which these data can be used to compute accurately the direction in which the instrument is pointed in terms of azimuth and elevation angles when it views the Moon. The difference between this direction and the computed direction of the Moon is taken to be the pointing error of the instrument. The technique has been applied to each of the three channels of all four CERES instruments using lunar observation data from 2006 to present. The maximum error was found to be 0.05 degrees in azimuth and 0.03. in elevation angle. This corresponds to an error in geolocation of 0.37 km near nadir. These results agree with those from the coastline detection method within one standard deviation for all but one case, where the difference was one-and-a-half standard deviations. The lunar and coastline techniques supplement each other for computing pixel location errors away from nadir. The alignment of the three channels in each instrument is evaluated as the differences of azimuth and elevation angles of the shortwave and window channels from those of the total channel. The alignment was within 0.1. for all cases and within 0.02. for most cases.
C1 [Daniels, Janet L.; Smith, G. Louis; Thomas, Susan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Priestley, Kory J.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23666 USA.
RP Daniels, JL (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM janet.l.daniels@nasa.gov; george.l.smith@nasa.gov;
kory.j.priestley@nasa.gov; susan.thomas-1@nasa.gov
FU Science Directorate of the Langley Research Center; Science Mission
Directorate of the Earth Science Division of NASA
FX The authors would like to thank the Science Directorate of the Langley
Research Center and the Science Mission Directorate of the Earth Science
Division of NASA for the support of the CERES Project.
NR 12
TC 0
Z9 0
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2016
VL 54
IS 1
BP 65
EP 73
DI 10.1109/TGRS.2015.2450182
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CW2PE
UT WOS:000364833900005
ER
PT J
AU Li, LH
Heymsfield, G
Carswell, J
Schaubert, DH
McLinden, ML
Creticos, J
Perrine, M
Coon, M
Cervantes, JI
Vega, M
Guimond, S
Tian, L
Emory, A
AF Li, Lihua
Heymsfield, Gerald
Carswell, James
Schaubert, Daniel H.
McLinden, Matthew L.
Creticos, Justin
Perrine, Martin
Coon, Michael
Cervantes, Jaime I.
Vega, Manuel
Guimond, Steve
Tian, Lin
Emory, Amber
TI The NASA High-Altitude Imaging Wind and Rain Airborne Profiler
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Clouds; dual-frequency; imaging; precipitation; radar; scanning; wind
ID TROPICAL CYCLONES; WEATHER RADAR; BAND RADARS; OCEAN; IWRAP
AB The High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP) is a dual-frequency (Ka- and Ku-bands), dual-beam (30 degrees and 40 degrees incidence angles), and conical scanning Doppler radar designed for operation on the NASA high-altitude (similar to 19 km) Global Hawk Unmanned Aerial System. HIWRAP was developed under the support of the NASA Instrument Incubator Program for studies of tropical storms and severe weather events. It utilizes solid-state transmitters along with a novel transmit and receive waveform scheme that results in a system with compact size, light weight, less power consumption, and lower cost compared to radars currently in use for precipitation and Doppler wind measurements. By combining volume backscattering measurements at Ku- and Ka-bands, HIWRAP is capable of imaging radar reflectivity and 3-D wind fields in clouds and precipitation. In addition, HIWRAP is also capable of measuring surface winds in an approach similar to SeaWinds on QuikSCAT. HIWRAP operating frequencies are similar to those used by the NASA Global Precipitation Measurement (GPM) Dual-frequency Precipitation Radar, making it suitable for providing airborne validation data for the GPM mission. This paper describes the scientific motivation for the development of HIWRAP as well as the system hardware, aircraft integration, and recent flight activities. Data from recent science flights are also presented.
C1 [Li, Lihua; Heymsfield, Gerald; McLinden, Matthew L.; Perrine, Martin; Coon, Michael; Vega, Manuel; Emory, Amber] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Carswell, James] Remote Sensing Solut, Barnstable, MA 02630 USA.
[Schaubert, Daniel H.] Univ Massachusetts, Amherst, MA 01003 USA.
[Creticos, Justin] Mitre Corp, Bedford, MA 01730 USA.
[Cervantes, Jaime I.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Guimond, Steve] Univ Maryland, College Pk, MD 20742 USA.
[Tian, Lin] Morgan State Univ, GESTAR, Baltimore, MD 21251 USA.
RP Li, LH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lihua.li@nasa.gov
FU NASA
FX The authors would like to thank the funding support from the NASA
Instrument Incubator Program during HIWRAP development, and supports
from the NASA Global Hawk, ER-2, and WB-57 groups during HIWRAP test
flights and field missions.
NR 28
TC 5
Z9 5
U1 6
U2 14
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2016
VL 54
IS 1
BP 298
EP 310
DI 10.1109/TGRS.2015.2456501
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CW2PE
UT WOS:000364833900023
ER
PT J
AU Kurth, WS
Hospodarsky, GB
Gurnett, DA
Lamy, L
Dougherty, MK
Nichols, J
Bunce, EJ
Pryor, W
Baines, K
Stallard, T
Melin, H
Crary, FJ
AF Kurth, W. S.
Hospodarsky, G. B.
Gurnett, D. A.
Lamy, L.
Dougherty, M. K.
Nichols, J.
Bunce, E. J.
Pryor, W.
Baines, K.
Stallard, T.
Melin, H.
Crary, F. J.
TI Saturn kilometric radiation intensities during the Saturn auroral
campaign of 2013
SO ICARUS
LA English
DT Article
DE Saturn, magnetosphere; Aurorae; Solar wind; Radio observations
ID COROTATING INTERACTION REGIONS; HUBBLE-SPACE-TELESCOPE; SOLAR-WIND;
RADIO-EMISSION; MAGNETIC-FIELD; MULTI-INSTRUMENT; EARTH; MAGNETOSPHERE;
DISTURBANCES; SIGNATURE
AB The Saturn auroral campaign carried out in the spring of 2013 used multiple Earth-based observations, remote-sensing observations from Cassini, and in situ-observations from Cassini to further our understanding of auroras at Saturn. Most of the remote sensing and Earth-based measurements are, by nature, not continuous. And, even the in situ measurements, while continuously obtained, are not always obtained in regions relevant to the study of the aurora. Saturn kilometric radiation, however, is remotely monitored nearly continuously by the Radio and Plasma Wave Science instrument on Cassini. This radio emission, produced by the cyclotron maser instability, is tightly tied to auroral processes at Saturn as are auroral radio emissions at other planets, most notably Jupiter and Earth. This paper provides the time history of the intensity of the radio emissions through the auroral campaign as a means of understanding the temporal relationships between the sometimes widely spaced observations of the auroral activity. While beaming characteristics of the radio emissions are known to prevent single spacecraft observations of this emission from being a perfect auroral activity indicator, we demonstrate a good correlation between the radio emission intensity and the level of UV auroral activity, when both measurements are available. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Kurth, W. S.; Hospodarsky, G. B.; Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Lamy, L.] Univ Paris Diderot, CNRS, LESIA, Observatoire Paris,UPMC, Meudon, France.
[Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, Technol & Med Space & Atmospher Phys Grp, Dept Phys, London SW7 28W, England.
[Nichols, J.; Bunce, E. J.; Stallard, T.; Melin, H.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Pryor, W.] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85128 USA.
[Baines, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Melin, H.] Space Environm Technol, Planetary & Space Sci Div, Pasadena, CA 91107 USA.
[Crary, F. J.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
RP Kurth, WS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM william-kurth@uiowa.edu
RI Nichols, Jonathan/F-5764-2010; Bunce, Emma/I-9067-2016;
OI Nichols, Jonathan/0000-0002-8004-6409; Bunce, Emma/0000-0002-9456-0345;
Hospodarsky, George/0000-0001-9200-9878; Stallard,
Tom/0000-0003-3990-670X; Kurth, William/0000-0002-5471-6202
FU NASA [1415150]; Jet Propulsion Laboratory; CNES; STFC Leicester
Consolidated Grant [ST/K001000/1]; Philip Leverhulme Award
FX Re-projected HST images are from the Auroral Planetary Imaging and
Spectroscopy (APIS) database (http://lesia.obspm.fr/apis) at
LESIA/VO-Paris Data Centre (Observatoire de Paris, CNRS). The research
at the University of Iowa was supported by NASA through Contract 1415150
with the Jet Propulsion Laboratory. The research in Meudon is supported
by CNES. EJB is supported by the STFC Leicester Consolidated Grant
ST/K001000/1, and a Philip Leverhulme Award.
NR 50
TC 0
Z9 0
U1 2
U2 11
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 JAN 1
PY 2016
VL 263
SI SI
BP 2
EP 9
DI 10.1016/j.icarus.2015.01.003
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU5WJ
UT WOS:000363602400002
ER
PT J
AU O'Donoghue, J
Melin, H
Stallard, TS
Provan, G
Moore, L
Badman, SV
Cowley, SWH
Baines, KH
Miller, S
Blake, JSD
AF O'Donoghue, James
Melin, Henrik
Stallard, Tom S.
Provan, G.
Moore, Luke
Badman, Sarah V.
Cowley, Stan W. H.
Baines, Kevin H.
Miller, Steve
Blake, James S. D.
TI Ground-based observations of Saturn's auroral ionosphere over three
days: Trends in HI temperature, density and emission with Saturn local
time and planetary period oscillation
SO ICARUS
LA English
DT Article
DE Saturn; Aurora; Magnetosphere; Ionosphere
ID CONJUGATE OBSERVATIONS; MAGNETIC-FIELD; H-3(+); CURRENTS; MAGNETOSPHERE;
ATMOSPHERES; NORTHERN; JUPITER; MODEL
AB On 19-21 April 2013, the ground-based 10-m W.M. Keck II telescope was used to simultaneously measure HI emissions from four regions of Saturn's auroral ionosphere: (1) the northern noon region of the main auroral oval; (2) the northern midnight main oval; (3) the northern polar cap and (4) the southern noon main oval. The H-3(+) emission from these regions was captured in the form of high resolution spectral images as the planet rotated. The results herein contain twenty-three H-3(+) temperatures, column densities and total emissions located in the aforementioned regions - ninety-two data points in total, spread over timescales of both hours and days. Thermospheric temperatures in the spring-time northern main oval are found to be cooler than their autumn-time southern counterparts by tens of K, consistent with the hypothesis that the total thermospheric heating rate is inversely proportional to magnetic field strength. The main oval H-3(+) density and emission is lower at northern midnight than it is at noon, in agreement with a nearby peak in the electron influx in the post-dawn sector and a minimum flux at midnight. Finally, when arranging the northern main oval H-3(+) parameters as a function of the oscillation period seen in Saturn's magnetic field the planetary period oscillation (PPO) phase - we see a large peak in H-3(+) density and emission at similar to 115 degrees northern phase, with a full-width at half-maximum (FWHM) of similar to 44 degrees. This seems to indicate that the influx of electrons associated with the PPO phase at 90 is responsible at least in part for the behavior of all H(3)(+)parameters. A combination of the H-3(+) production and loss timescales and the 10 uncertainty in the location of a given PPO phase are likely, at least in part, to be responsible for the observed peaks in H-3(+) density and emission occurring at a later time than the peak precipitation expected at 90 PPO phase. (C) 2015 Elsevier Inc. All rights reserved.
C1 [O'Donoghue, James; Melin, Henrik; Stallard, Tom S.; Provan, G.; Cowley, Stan W. H.; Blake, James S. D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Miller, Steve] UCL, Dept Phys & Astron, Atmospher Phys Lab, London WC1E 6BT, England.
[Baines, Kevin H.] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[O'Donoghue, James; Moore, Luke] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Badman, Sarah V.] Univ Lancaster, Dept Phys, Lancaster LA1 4YW, England.
RP O'Donoghue, J (reprint author), Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
OI Stallard, Tom/0000-0003-3990-670X
FU UK Science and Technology Facilities Council (STFC); Royal Astronomical
Society Research Fellowship; National Aeronautics and Space
Administration [9500303356]
FX 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 NASA. We are
particularly grateful to the observing staff in both Waimea and Mauna
Kea for their kind assistance and we praise their ability to seemingly
clear the sky of clouds whenever we observe. The observations were made
to support the Cassini auroral campaign in April 2013. Discussions
within the international team lead by Tom Stallard on 'Comparative
Jovian Aeronomy' have greatly benefited this work; this was hosted by
the International Space Science Institute (ISSI). The UK Science and
Technology Facilities Council (STFC) supported this work through the
Studentship Enhancement Programme (STEP) for J.O'D. and consolidated
grant support for T.S.S., S.W.H.C. and H.M., whilst S.V.B. was supported
by a Royal Astronomical Society Research Fellowship. This material is
based upon work supported by the National Aeronautics and Space
Administration under Grant No. 9500303356 issued through the Planetary
Astronomy Program for L.M. and J.O'D. We thank the NASA Planetary Data
System (PDS) for planetary parameter and viewing geometry data.
NR 58
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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 JAN 1
PY 2016
VL 263
SI SI
BP 44
EP 55
DI 10.1016/j.icarus.2015.04.018
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU5WJ
UT WOS:000363602400006
ER
PT J
AU Melin, H
Badman, SV
Stallard, TS
Cowley, SWH
Dyudina, U
Nichols, JD
Provan, G
O'Donoghue, J
Pryor, WR
Baines, KH
Miller, S
Gustin, J
Radioti, A
Tao, C
Meredith, CJ
Blake, JSD
Johnson, RE
AF Melin, Henrik
Badman, S. V.
Stallard, T. S.
Cowley, S. W. H.
Dyudina, U.
Nichols, J. D.
Provan, G.
O'Donoghue, J.
Pryor, W. R.
Baines, K. H.
Miller, S.
Gustin, J.
Radioti, A.
Tao, C.
Meredith, C. J.
Blake, J. S. D.
Johnson, R. E.
TI Simultaneous multi-scale and multi-instrument observations of Saturn's
aurorae during the 2013 observing campaign
SO ICARUS
LA English
DT Article
DE Saturn, atmosphere; Magnetosphere; Aeronomy
ID HUBBLE-SPACE-TELESCOPE; H-3(+) INFRARED-EMISSION; RADIO ROTATION PERIOD;
KECK-II TELESCOPE; MAGNETIC-FIELD; ECHELLE SPECTROGRAPH;
UPPER-ATMOSPHERE; GIANT PLANETS; ULTRAVIOLET; IONOSPHERE
AB On 21 April 2013, during a co-ordinated Saturn auroral observing campaign, the northern and southern poles of the planet were observed from the Earth using the NASA Infrared Telescope Facility (IRTF), Keck, and Hubble Space Telescope (HST) simultaneously with the Cassini infrared, visible, and ultraviolet remote sensing instruments. We present simultaneous multi-scale and multi-wavelength analysis of the morphology of auroral emissions at Saturn. The visible main auroral emission vary between similar to 2 and 10 kR on timescales of minutes and across spatial scales of down to similar to 14 km on the planet. The H-2 Far Ultraviolet (FUV) brightness varies by a factor of similar to 10, from similar to 4-40 kR, over timescales of 1 min and spatial scales of 720 km. H-3(+) infrared emissions vary less than the H-2 emissions, from similar to 5-10 mu W m(-2) sr(-1), over similar spatial scales (similar to 300 km) and timescales of a few seconds to a few hours. The fine-scale temporal and spatial features seen in the main oval show that complex structures are present even during quiet solar wind conditions. Diffuse ultraviolet emissions southward of the southern midnight main oval that are not seen in the infrared, implying a steep temperature gradient of similar to 50 K over 2-4 degrees latitude equatorward of the main oval. Dynamics on scales of similar to 100 km at the poles are revealed by lower spatial resolution observations, the morphologies of which are partly consistent with overlapping local-time fixed and co-rotating current systems. We also present the first direct comparison of simultaneous infrared, visible, and ultraviolet auroral emissions at Saturn. Finally, the main auroral emissions are found to be approximately co-located in the midnight sector, forming an arc with a width of similar to 0.5-1 degrees, at 72-74 degrees southern latitude, moving slightly equatorward with increasing local-time. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Melin, Henrik; Stallard, T. S.; Cowley, S. W. H.; Nichols, J. D.; Provan, G.; Meredith, C. J.; Blake, J. S. D.; Johnson, R. E.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Melin, Henrik] Space Environm Technol, Pacific Palisades, CA 90272 USA.
[Badman, S. V.] Univ Lancaster, Dept Phys, Lancaster LA1 4YW, England.
[Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miller, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[O'Donoghue, J.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Pryor, W. R.] Cent Arizona Coll, Coolidge, AZ 85128 USA.
[Gustin, J.; Radioti, A.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Tao, C.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31000 Toulouse, France.
[Dyudina, U.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Melin, H (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM hpm5@leicester.ac.uk
RI Nichols, Jonathan/F-5764-2010;
OI Nichols, Jonathan/0000-0002-8004-6409; Stallard, Tom/0000-0003-3990-670X
FU UK STFC [ST/K001000/1]; Royal Astronomical Society Research Fellowship;
SET by NASA CDAP grant [NNX-13AG41G]; STFC Advanced Fellowship; STFC
studentships; PRODEX program; Belgian Federal Science Policy Office
(BELSPO); NASA Cassini project
FX Part 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
NASA. This work includes observations made with the NASA/ESA Hubble
Space Telescope, obtained at the Space Telescope Science Institute,
which is operated by AURA, Inc. for NASA. The observations were obtained
during HST program GO 13051. HM, TSS, JO'D, JSDB, and REJ are visiting
Astronomers at the Infrared Telescope Facility, which is operated by the
University of Hawaii under Cooperative Agreement No. NNX-08AE38A with
the NASA, Science Mission Directorate, Planetary Astronomy Program. This
work was supported by the UK STFC Grant ST/K001000/1 for HM, TSS, SWHC,
and GP, a Royal Astronomical Society Research Fellowship for SVB, and at
SET by NASA CDAP grant NNX-13AG41G. JDN was supported by an STFC
Advanced Fellowship. JO'D, JSDB, CJM, and REJ were supported by STFC
studentships. JG is supported by the PRODEX program in collaboration
with the Belgian Federal Science Policy Office (BELSPO). UD was
supported by the NASA Cassini project. We thank G. M. Holsclaw for
supplying the time-dependent UVIS calibration curves.
NR 87
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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 JAN 1
PY 2016
VL 263
SI SI
BP 56
EP 74
DI 10.1016/j.icarus.2015.08.021
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU5WJ
UT WOS:000363602400007
ER
PT J
AU Badman, SV
Provan, G
Bunce, EJ
Mitchell, DG
Melin, H
Cowley, SWH
Radioti, A
Kurth, WS
Pryor, WR
Nichols, JD
Jinks, SL
Stallard, TS
Brown, RH
Baines, KH
Dougherty, MK
AF Badman, S. V.
Provan, G.
Bunce, E. J.
Mitchell, D. G.
Melin, H.
Cowley, S. W. H.
Radioti, A.
Kurth, W. S.
Pryor, W. R.
Nichols, J. D.
Jinks, S. L.
Stallard, T. S.
Brown, R. H.
Baines, K. H.
Dougherty, M. K.
TI Saturn's auroral morphology and field-aligned currents during a solar
wind compression
SO ICARUS
LA English
DT Article
DE Saturn, magnetosphere; Aurorae; Solar wind
ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOSPHERIC DYNAMICS; PRESSURE;
EMISSION; JUPITER; REGIONS; STORMS; RADIO; EARTH; OVAL
AB On 21-22 April 2013, during a coordinated auroral observing campaign, instruments onboard Cassini and the Hubble Space Telescope observed Saturn's aurora while Cassini traversed Saturn's high latitude auroral field lines. Signatures of upward and downward field-aligned currents were detected in the nightside magnetosphere in the magnetic field and plasma measurements. The location of the upward current corresponded to the bright ultraviolet auroral arc seen in the auroral images, and the downward current region was located poleward of the upward current in an aurorally dark region. Within the polar cap magnetic field and plasma fluctuations were identified with periods of similar to 20 and similar to 60 min. The northern and southern auroral ovals were observed to rock in latitude in phase with the respective northern and southern planetary period oscillations. A solar wind compression impacted Saturn's magnetosphere at the start of 22 April 2013, identified by an intensification and extension to lower frequencies of the Saturn kilometric radiation, with the following sequence of effects: (1) intensification of the auroral field-aligned currents; (2) appearance of a localised, intense bulge in the dawnside (04-06 LT) aurora while the midnight sector aurora remained fainter and narrow; and (3) latitudinal broadening and poleward contraction of the nightside aurora, where the poleward motion in this sector is opposite to that expected from a model of the auroral oval's usual oscillation. These observations are interpreted as the response to tail reconnection events, initially involving Vasyliunas-type reconnection of closed mass-loaded magnetotail field lines, and then proceeding onto open lobe field lines, causing the contraction of the polar cap region on the night side. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Badman, S. V.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
[Provan, G.; Bunce, E. J.; Melin, H.; Cowley, S. W. H.; Nichols, J. D.; Jinks, S. L.; Stallard, T. S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Mitchell, D. G.] JHU APL, Laurel, MD 20723 USA.
[Melin, H.] Space Environm Technol, Los Angeles, CA USA.
[Radioti, A.] Univ Liege, LPAP, B-4000 Liege, Belgium.
[Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Pryor, W. R.] Cent Arizona Coll, Coolidge, AZ 85128 USA.
[Brown, R. H.] Univ Arizona, LPL, Tucson, AZ 85721 USA.
[Baines, K. H.] JPL, Pasadena, CA 91109 USA.
[Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England.
RP Badman, SV (reprint author), Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
EM s.badman@lancaster.ac.uk
RI Nichols, Jonathan/F-5764-2010; Bunce, Emma/I-9067-2016;
OI Nichols, Jonathan/0000-0002-8004-6409; Bunce, Emma/0000-0002-9456-0345;
Stallard, Tom/0000-0003-3990-670X; Kurth, William/0000-0002-5471-6202
FU Royal Astronomical Society Research Fellowship; STFC [ST/K001000/1,
ST/1004084/1]; Philip Leverhulme Award; NASA Office of Space Science
[NAS5-97271]; NASA [1415150]; Jet Propulsion Laboratory
FX This work uses observations with the NASA/ESA Hubble Space Telescope
obtained at the Space Telescope Science Institute (STScI), which is
operated by AURA, Inc. for NASA. SVB was supported by a Royal
Astronomical Society Research Fellowship. EJB, GP, HM, SWHC and TSS were
supported by STFC grant ST/K001000/1, and EJB by a Philip Leverhulme
Award. SLJ was supported by an STFC PhD studentship and JDN by an STFC
Advanced Fellowship (ST/1004084/1). DGM was supported by the NASA Office
of Space Science under Task Order 003 of contract NAS5-97271 between
NASA Goddard Space Flight Center and the Johns Hopkins University. The
research at the University of Iowa was supported by NASA through
contract 1415150 with the Jet Propulsion Laboratory.
NR 74
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U1 1
U2 16
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 JAN 1
PY 2016
VL 263
SI SI
BP 83
EP 93
DI 10.1016/j.icarus.2014.11.014
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU5WJ
UT WOS:000363602400009
ER
PT J
AU Yasunari, TJ
Colarco, PR
Lau, WKM
Osada, K
Kido, M
Mahanama, SPP
Kim, KM
da Silva, AM
AF Yasunari, Teppei J.
Colarco, Peter R.
Lau, William K. M.
Osada, Kazuo
Kido, Mizuka
Mahanama, Sarith P. P.
Kim, Kyu-Myong
da Silva, Arlindo M.
TI Total dust deposition flux during precipitation in Toyama, Japan, in the
spring of 2009: A sensitivity analysis with the NASA GEOS-5 Model
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Dust; Wet deposition; Numerical modeling; Japan; Precipitation; Aerosol
ID AEROSOL OPTICAL-THICKNESS; ASIAN DUST; MINERAL DUST; FIELD CAMPAIGN;
NORTH PACIFIC; GOCART MODEL; EARTH SYSTEM; WET DEPOSITION; DRY
DEPOSITION; SOIL DUST
AB We compared the observed total dust deposition fluxes during precipitation (TDP) mainly at Toyama in Japan during the period January-April 2009 with results available from four NASA GEOS-5 global model experiments. The modeled results were obtained from three previous experiments and carried out in one experiment, which were all driven by assimilated meteorology and simulating aerosol distributions for the time period. We focus mainly on the observations of two distinct TDP events, which were reported in Osada et al. (2011), at Toyama, Japan, in February (Event B) and March 2009 (Event C). Although all of our GEOS-5 simulations captured aspects of the observed TDP, we found that our low horizontal spatial resolution control experiment performed generally the worst The other three experiments were run at a higher spatial resolution, with the first differing only in that respect from the control, the second adding imposed a prescribed corrected precipitation product, and the final experiment adding as well assimilation of aerosol optical depth based on MODIS observations. During Event C, the increased horizontal resolution could increase TDP with precipitation increase. There was no significant improvement, however, due to the imposition of the corrected precipitation product. The simulation that incorporated aerosol data assimilation performed was by far the best for this event, but even so could only reproduce less than half of the observed TDP despite the significantly increased atmospheric dust mass concentrations. All three of the high spatial resolution experiments had higher simulated precipitation at Toyama than was observed and that in the lower resolution control run. During Event B, the aerosol data assimilation run did not perform appreciably better than the other higher resolution simulations, suggesting that upstream conditions (i.e., upstream cloudiness), or vertical or horizontal misplacement of the dust plume did not allow for significant improvement in the simulated aerosol distributions. Furthermore, a detailed comparison of observed hourly precipitation and surface particulate mass concentration data suggests that the observed TDP during Event B was highly dependent on short periods of weak precipitation correlated with elevated dust surface concentrations, important details possibly not captured well in a current global model. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Yasunari, Teppei J.] Univ Space Res Assoc, Goddard Earth Sci & Technol & Res, Columbia, MD 21046 USA.
[Yasunari, Teppei J.; Colarco, Peter R.; Lau, William K. M.; Mahanama, Sarith P. P.; Kim, Kyu-Myong; da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lau, William K. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Osada, Kazuo] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan.
[Kido, Mizuka] Toyama Prefectural Environm Sci Res Ctr, Kosugi, Toyama 9390363, Japan.
[Mahanama, Sarith P. P.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Yasunari, TJ (reprint author), Hokkaido Univ, Fac Engn, Sapporo, Hokkaido 0608628, Japan.
EM t.j.yasunari@eng.hokudai.ac.jp
RI Lau, William /E-1510-2012; Colarco, Peter/D-8637-2012; Yasunari,
Teppei/E-5374-2010
OI Lau, William /0000-0002-3587-3691; Colarco, Peter/0000-0003-3525-1662;
Yasunari, Teppei/0000-0002-9896-9404
FU Science Mission Directorate at NASA Headquarters; NASA's MAP program
FX The Science Mission Directorate at NASA Headquarters supported this
study by the Aqua Terra Science Program and the Modeling, Analysis, and
Prediction (MAP) Program. The GEOS-5 model development and the MERRAero
project in the Global Modeling and Assimilation Office were also funded
by NASA's MAP program. The GEOS-5 simulations were carried out in the
system for NASA Center for Climate Simulation (NCCS). Max Suarez (NASA),
Larry Takacs (SSAI), and Randy Koster (NASA), at NASA Goddard Space
Flight Center (NASA/GSFC) kindly helped coding in GEOS-5, giving us
useful information to understand GEOS-5 more, and had useful discussions
on the model. Ravi Govindaraju (SSAI) helped the treatment of the
outputs from the EXP4 GEOS-5 experiment (MERRAero). Useful comments and
suggestions were provided by Anton Darmenov (NASA), Qian Tan
(GESTAR/USRA), and Tetsuzo Yasunari (Research Institute for Humanity and
Nature: RIHN) respectively. The lidar data at TESC maintained by NIES
were used with helpful information provided by Atsushi Shimizu and Nobuo
Sugimoto (NIES). The SPM data in Toyama were provided by TESC in Toyama
prefecture. The authors gratefully acknowledge the NOAA Air Resources
Laboratory (ARL) for the provision of the HYSPLIT transport and
dispersion model and/or READY website (http://ready.arl.noaa.gov) used
in this publication. Google Earth was used for distance calculation. Jan
Angevine (ARTS) at NASA/GSFC proofread this paper.
NR 83
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD JAN 1
PY 2016
VL 167
BP 298
EP 313
DI 10.1016/j.atmosres.2015.08.005
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2CJ
UT WOS:000362609300025
ER
PT J
AU Aleksic, J
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Bangale, P
Barcelo, M
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Biland, A
Bitossi, M
Blanch, O
Bonnefoy, S
Bonnolic, G
Borracci, F
Bretzl, T
Carmona, E
Carosi, A
Cecchi, R
Colin, P
Colombo, E
Contreras, JL
Corti, D
Cortina, J
Covino, S
Da Vela, P
Dazzi, F
De Angelis, A
De Caneva, G
De Lotto, B
Wilhelmi, ED
Mendez, CD
Dettlaff, A
Prester, DD
Dorner, D
Doro, M
Einecke, S
Eisenacher, D
Elsaesser, D
Fidalgo, D
Fink, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Giavitto, G
Godinovic, N
Munoz, AG
Gozzini, SR
Haberer, W
Hadasch, D
Hanabata, Y
Hayashida, M
Herrera, J
Hildebrand, D
Hose, J
Hrupec, D
Idec, W
Illa, JM
Kadenius, V
Kellermann, H
Knoetig, ML
Kodani, K
Konno, Y
Krause, J
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lemus, JL
Lewandowska, N
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorca, A
Lorenz, E
Lozano, I
Makariev, M
Mallot, K
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Munar-Adrover, P
Nakajima, D
Negrello, M
Neustroev, V
Niedzwiecki, A
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Rugamer, S
Saito, T
Saito, K
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schlammer, J
Schmidl, S
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Spanier, E
Stamerra, A
Steinbring, T
Storz, J
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Tejedor, LA
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Tibolla, O
Torres, DF
Toyama, T
Treves, A
Vogler, P
Wetteskind, H
Will, M
Zanin, R
AF Aleksic, J.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Bangale, P.
Barcelo, M.
Barrio, J. A.
Gonzalez, J. Becerra
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Biland, A.
Bitossi, M.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretzl, T.
Carmona, E.
Carosi, A.
Cecchi, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Corti, D.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Caneva, G.
De Lotto, B.
de Ona Wilhelmi, E.
Delgado Mendez, C.
Dettlaff, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Eisenacher, D.
Elsaesser, D.
Fidalgo, D.
Fink, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Garcia Lopez, R. J.
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giavitto, G.
Godinovic, N.
Gonzalez Munoz, A.
Gozzini, S. R.
Haberer, W.
Hadasch, D.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hildebrand, D.
Hose, J.
Hrupec, D.
Idec, W.
Illa, J. M.
Kadenius, V.
Kellermann, H.
Knoetig, M. L.
Kodani, K.
Konno, Y.
Krause, J.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lemus, J. L.
Lewandowska, N.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorca, A.
Lorenz, E.
Lozano, I.
Makariev, M.
Mallot, K.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Munar-Adrover, P.
Nakajima, D.
Negrello, M.
Neustroev, V.
Niedzwiecki, A.
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Reinthal, R.
Rhode, W.
Ribo, M.
Rico, J.
Garcia, J. Rodriguez
Ruegamer, S.
Saito, T.
Saito, K.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schultz, C.
Schlammer, J.
Schmidl, S.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Spanier, E.
Stamerra, A.
Steinbring, T.
Storz, J.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Tejedor, L. A.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Tibolla, O.
Torres, D. F.
Toyama, T.
Treves, A.
Vogler, P.
Wetteskind, H.
Will, M.
Zanin, R.
TI The major upgrade of the MAGIC telescopes, Part II: A performance study
using observations of the Crab Nebula
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Gamma-ray astronomy; Cherenkov telescopes; Crab Nebula
ID GAMMA-RAY EMISSION; CHERENKOV TELESCOPES; MONTE-CARLO; PULSAR; SYSTEM;
FLARES; ARRAYS; IMAGES; TEV
AB MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located in the Canary island of La Palma, Spain. During summer 2011 and 2012 it underwent a series of upgrades, involving the exchange of the MAGIC-I camera and its trigger system, as well as the upgrade of the readout system of both telescopes. We use observations of the Crab Nebula taken at low and medium zenith angles to assess the key performance parameters of the MAGIC stereo system. For low zenith angle observations, the standard trigger threshold of the MAGIC telescopes is similar to 50 GeV. The integral sensitivity for point-like sources with Crab Nebula-like spectrum above 220 GeV is (0.66 +/- 0.03)% of Crab Nebula flux in 50 h of observations. The angular resolution, defined as the a of a 2-dimensional Gaussian distribution, at those energies is less than or similar to 0.07 degrees, while the energy resolution is 16%. We also re-evaluate the effect of the systematic uncertainty on the data taken with the MAGIC telescopes after the upgrade. We estimate that the systematic uncertainties can be divided in the following components: < 15% in energy scale, 11%-18% in flux normalization and +/- 0.15 for the energy spectrum power-law slope. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Aleksic, J.; Barcelo, M.; Blanch, O.; Cortina, J.; Giavitto, G.; Gonzalez Munoz, A.; Hadasch, D.; Illa, J. M.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.] IFAE, E-08193 Barcelona, Spain.
[Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Longo, F.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; 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, INFN Pisa, I-53100 Siena, Italy.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Zagreb, Croatia.
[Bangale, P.; Borracci, F.; Colin, P.; Dazzi, F.; Dettlaff, A.; Fink, D.; Fruck, C.; Haberer, W.; Hose, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Noda, K.; Paneque, D.; Garcia, J. Rodriguez; Schlammer, J.; Schmidl, S.; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Wetteskind, H.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fidalgo, D.; Fonseca, M. V.; Lemus, J. L.; Lopez, M.; Lorca, A.; Lozano, I.; Satalecka, K.; Scapin, V.; Tejedor, L. A.] Univ Complutense, E-28040 Madrid, Spain.
[Gonzalez, J. Becerra; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Tescaro, D.; Will, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; De Caneva, G.; Garczarczyk, M.; Giavitto, G.; Gozzini, S. R.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Hildebrand, D.; Knoetig, M. L.; Prandini, E.; Vogler, P.] ETH, CH-8093 Zurich, Switzerland.
[Bretzl, T.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Ruegamer, S.; Spanier, E.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97070 Wurzburg, Germany.
[Carmona, E.; Delgado Mendez, C.] CIEMAT, E-28040 Madrid, Spain.
[de Ona Wilhelmi, E.; Hadasch, D.] Inst Space Sci, E-08193 Barcelona, Spain.
[Corti, D.; Doro, M.; Mariotti, M.; Negrello, M.; Paiano, S.; Scalzotto, V.; Schultz, C.] Univ Padua, Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, CERES IEEC, Unitat Fis Radiac, E-08193 Barcelona, Spain.
[Galindo, D.; Marcote, B.; Munar-Adrover, P.; 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.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan.
[Kadenius, V.; Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, Univ Turku, Finnish MAGIC Consortium,Tuorla Observ, SF-90100 Oulu, Finland.
[Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, INFN Pisa, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, Inst Space Sci, E-08193 Barcelona, Spain.
[Treves, A.] Univ Insubria, INFN Milano Bicocca, I-22100 Como, Italy.
[Bitossi, M.] European Gravitat Observ, I-56021 S Stefano A Macerata, Italy.
[Cecchi, R.] Univ Siena, INFN Siena, I-53100 Siena, Italy.
[Gonzalez, J. Becerra] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bretzl, T.] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland.
[Hadasch, D.; Nilsson, K.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Lindfors, E.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Mankuzhiyil, N.] Bhabha Atom Res Ctr, Astrophys Sci Div, Bombay 400085, Maharashtra, India.
[Persic, M.] INAF Trieste, Trieste, Italy.
RP Carmona, E (reprint author), CIEMAT, E-28040 Madrid, Spain.
EM emiliano.carmona@ciemat.es; jsitarek@uni.lodz.pl
RI Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; Fonseca Gonzalez,
Maria Victoria/I-2004-2015; Miranda, Jose Miguel/F-2913-2013; Tejedor,
Luis/N-5494-2014; Poutanen, Juri/H-6651-2016; Font, Lluis/L-4197-2014;
Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya,
Marcos/L-2304-2014; Temnikov, Petar/L-6999-2016; Maneva,
Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Delgado,
Carlos/K-7587-2014; Torres, Diego/O-9422-2016; GAug, Markus/L-2340-2014;
OI Doro, Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507;
de Ona Wilhelmi, Emma/0000-0002-5401-0744; Bonnoli,
Giacomo/0000-0003-2464-9077; Mazin, Daniel/0000-0002-2010-4005; Barrio,
Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Stamerra,
Antonio/0000-0002-9430-5264; Prada Moroni, Pier
Giorgio/0000-0001-9712-9916; Antonelli, Lucio
Angelo/0000-0002-5037-9034; LA BARBERA, ANTONINO/0000-0002-5880-8913;
Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto,
Barbara/0000-0003-3624-4480; Persic, Massimo/0000-0003-1853-4900;
Miranda, Jose Miguel/0000-0002-1472-9690; Tejedor,
Luis/0000-0003-1525-9085; Poutanen, Juri/0000-0002-0983-0049; Font,
Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose
Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908;
Temnikov, Petar/0000-0002-9559-3384; Delgado,
Carlos/0000-0002-7014-4101; Torres, Diego/0000-0002-1522-9065; GAug,
Markus/0000-0001-8442-7877; Prandini, Elisa/0000-0003-4502-9053; Becerra
Gonzalez, Josefa/0000-0002-6729-9022
FU German BMBF; German MPG; Italian INFN; Swiss National Fund SNF; Spanish
MINECO [FPA2012-39502, JCI-2011-10019]; CPAN [CSD2007-00042]; Spanish
Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland
[127740]; DFG Cluster of Excellence "Origin and Structure of the
Universe"; Croatian Science Foundation (HrZZ) Project [09/176]; DFG
Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW
grant [745/N-HESS-MAGIC/2010/0]; ERDF
FX We would like to thank the Instituto de Astrofisica de Canarias for the
excellent working conditions at the Observatorio del Roque de los
Muchachos in La Palma. The support of the German BMBF and MPG, the
Italian INFN, the Swiss National Fund SNF, and the Spanish MINECO is
gratefully acknowledged. This work was also supported by CPAN
CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish
Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of
Finland, by the DFG Cluster of Excellence "Origin and Structure of the
Universe", by the Croatian Science Foundation (HrZZ) Project 09/176, by
the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by
the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. J. S. is supported by
ERDF and Spanish MINECO through FPA2012-39502 and JCI-2011-10019 grants.
We thank the two anonymous referees for their comments which helped to
improve the paper.
NR 49
TC 26
Z9 26
U1 4
U2 25
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 JAN
PY 2016
VL 72
BP 76
EP 94
DI 10.1016/j.astropartphys.2015.02.005
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CS5UE
UT WOS:000362143000008
ER
PT J
AU Theis, ML
Candian, A
Tielens, AGGM
Lee, TJ
Fortenberry, RC
AF Theis, Mallory L.
Candian, Alessandra
Tielens, Alexander G. G. M.
Lee, Timothy J.
Fortenberry, Ryan C.
TI Electronically Excited States of Anisotropically Extended
Singly-Deprotonated PAH Anions
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBONS; ACETALDEHYDE ENOLATE ANION; DIFFUSE
INTERSTELLAR BANDS; COUPLED-CLUSTER METHOD; DIPOLE-BOUND ANIONS;
BASIS-SETS; INFRARED-SPECTRA; AUTODETACHMENT SPECTROSCOPY; MOLECULAR
ANION; CH2CN
AB Polycyclic aromatic hydrocarbons (PAHs) play a significant role in the chemistry of the interstellar medium (ISM) as well as in hydrocarbon combustion. These molecules can have high levels of diversity with the inclusion of heteroatoms and the addition or removal of hydrogens to form charged or radical species. There is an abundance of data on the cationic forms of these molecules, but there have been many fewer studies on the anionic species. The present study focuses on the anionic forms of deprotonated PAHs. It has been shown in previous work that PAHs containing nitrogen heteroatoms (PANHs) have the ability to form valence excited states giving anions electronic absorption features. This work analyzes how the isoelectronic pure PAHs behave under similar structural constructions. Singly deprotonated forms of benzene, naphthalene, anthracene, and tetracene classes are examined. None of the neutral-radicals possess dipole moments large enough to support dipole-bound excited states in their corresponding closed-shell anions. Even though the PANH anion derivatives support valence excited states for three-ringed structures, it is not until four-ringed structures of the pure PAR anion derivatives that valence excited states are exhibited. However, anisotropically extended PAHs larger than tetracene will likely exhibit valence excited states. The relative energies for the anion isomers are very small for all of the systems in this study.
C1 [Theis, Mallory L.; Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
[Candian, Alessandra; Tielens, Alexander G. G. M.] Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Theis, Mallory L.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA.
RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
EM rfortenberry@georgiasouthern.edu
RI Lee, Timothy/K-2838-2012
FU Georgia Southern University; European Research Council [246976];
National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH13ZDA017C]
FX The work undertaken by M.L.T. and R.C.F. is supported by start-up funds
provided by Georgia Southern University. European Research Council Grant
246976 supports work on interstellar PAHs done at Leiden Observatory.
This material is based upon work supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice NNH13ZDA017C issued through the Science
Mission Directorate. The figures are produced with the CheMVP program
developed at the Center for Computational Quantum Chemistry at the
University of Georgia, and the MOs in Figure 4 are created through the
WebMO computational chemistry graphical user interface (ref 75).
NR 74
TC 1
Z9 1
U1 4
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD DEC 31
PY 2015
VL 119
IS 52
BP 13048
EP 13054
DI 10.1021/acs.jpca.5b10421
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DA3NW
UT WOS:000367705400016
PM 26645382
ER
PT J
AU Fuchs, EC
Bitschnau, B
Wexler, AD
Woisetschlager, J
Freund, FT
AF Fuchs, Elmar C.
Bitschnau, Brigitte
Wexler, Adam D.
Woisetschlaeger, Jakob
Freund, Friedemann T.
TI A Quasi-Elastic Neutron Scattering Study of the Dynamics of Electrically
Constrained Water
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID BRIDGE; VIBRATIONS; LIQUIDS; ENERGY; PROTON; FIELD; ICE; ION
AB We have measured the quasi-elastic neutron scattering (QENS) of an electrohydrodynamic liquid bridge formed between two beakers of pure water when a high voltage is applied, a setup allowing to investigate water under high-voltage without high currents. From this experiment two proton populations were distinguished: one consisting of protons strongly bound to oxygen atoms (immobile population, elastic component) and a second one of quasi-free protons (mobile population, inelastic component) both detected by QENS. The diffusion coefficient of the quasi-free protons was found to be D = (26 +/- 10) x 10(-5) cm(2) s(-1) with a jump length l(av) similar to 3 angstrom and an average residence time of tau(0) = 0.55 +/- 0.08 ps. The associated proton mobility in the proton channel of the bridge is similar to 9.34 x 10(-7) m(2) V-1 s(-1), twice as fast as diffusion-based proton mobility in bulk water. It also matches the so-called electrohydrodynamic or "apparent" charge mobility, an experimental quantity which so far has lacked molecular interpretation. These results further corroborate the proton channel model for liquid water under high voltage and give new insights into the molecular mechanisms behind electrohydrodynamic charge transport phenomena and delocalization of protons in liquid water.
C1 [Fuchs, Elmar C.; Wexler, Adam D.] Wetsus European Ctr Excellence Sustainable Water, NL-8900 CC Leeuwarden, Netherlands.
[Bitschnau, Brigitte] Graz Univ Technol, Inst Phys & Theoret Chem, A-8010 Graz, Austria.
[Woisetschlaeger, Jakob] Graz Univ Technol, Inst Thermal Turbomachinery & Machine Dynam, Working Grp Metrol Laser Opt Metrol, A-8010 Graz, Austria.
[Freund, Friedemann T.] NASA, Ames Res Ctr, NASA Program, Moffett Field, CA 94035 USA.
[Freund, Friedemann T.] NASA, Ames Res Ctr, Projects Div PX, Moffett Field, CA 94035 USA.
[Freund, Friedemann T.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
RP Fuchs, EC (reprint author), Wetsus European Ctr Excellence Sustainable Water, Agora 1, NL-8900 CC Leeuwarden, Netherlands.
EM elmar.fuchs@wetsus.nl
OI Woisetschlaeger, Jakob/0000-0002-7057-761X
FU Dutch Ministry of Economic Affairs; Ministry of Infrastructure and
Environment; Province of Fryslan; Northern Netherlands Provinces
FX This work was performed at Wetsus, European Centre of Excellence for
Sustainable Water Technology and at Laboratoire Leon Brillouin, Saclay,
France. Wetsus is cofunded by the Dutch Ministry of Economic Affairs and
Ministry of Infrastructure and Environment, the Province of Fryslan, and
the Northern Netherlands Provinces. The authors thank the participants
of the research theme "Applied Water Physics" for the fruitful
discussions and their financial support. They furthermore thank Jose
Teixeira and the team at LLB for help and support.
NR 38
TC 3
Z9 3
U1 3
U2 12
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD DEC 31
PY 2015
VL 119
IS 52
BP 15892
EP 15900
DI 10.1021/acs.jpcb.5b10751
PG 9
WC Chemistry, Physical
SC Chemistry
GA DA3NU
UT WOS:000367705200013
PM 26643863
ER
PT J
AU Skiles, SM
Painter, TH
Belnap, J
Holland, L
Reynolds, RL
Goldstein, HL
Lin, J
AF Skiles, S. McKenzie
Painter, Thomas H.
Belnap, Jayne
Holland, Lacey
Reynolds, Richard L.
Goldstein, Harland L.
Lin, John
TI Regional variability in dust-on-snow processes and impacts in the Upper
Colorado River Basin
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snow energy balance; snowmelt; dust-on-snow; light absorbing impurities;
snow hydrology; spatial variability
ID WIND EROSION; CLIMATE; COVER; DEPOSITION; HYDROLOGY; PLATEAU; BALANCE;
ENERGY; MODEL; UTAH
AB Dust deposition onto mountain snow cover in the Upper Colorado River Basin frequently occurs in the spring when wind speeds and dust emission peaks on the nearby Colorado Plateau. Dust loading has increased since the intensive settlement in the western USA in the mid 1880s. The effects of dust-on-snow have been well studied at Senator Beck Basin Study Area (SBBSA) in the San Juan Mountains, CO, the first high-altitude area of contact for predominantly southwesterly winds transporting dust from the southern Colorado Plateau. To capture variability in dust transport from the broader Colorado Plateau and dust deposition across a larger area of the Colorado River water sources, an additional study plot was established in 2009 on Grand Mesa, 150 km to the north of SBBSA in west central, CO. Here, we compare the 4-year (2010-2013) dust source, deposition, and radiative forcing records at Grand Mesa Study Plot (GMSP) and Swamp Angel Study Plot (SASP), SBBSA's subalpine study plot. The study plots have similar site elevations/environments and differ mainly in the amount of dust deposited and ensuing impacts. At SASP, end of year dust concentrations ranged from 0.83 mg g(-1) to 4.80 mg g(-1), and daily mean spring dust radiative forcing ranged from 50-65Wm(-2), advancing melt by 24-49 days. At GMSP, which received 1.0 mg g(-1) less dust per season on average, spring radiative forcings of 32-50Wm(-2) advanced melt by 15-30 days. Remote sensing imagery showed that observed dust events were frequently associated with dust emission from the southern Colorado Plateau. Dust from these sources generally passed south of GMSP, and back trajectory footprints modelled for observed dust events were commonly more westerly and northerly for GMSP relative to SASP. These factors suggest that although the southern Colorado Plateau contains important dust sources, dust contributions from other dust sources contribute to dust loading in this region, and likely account for the majority of dust loading at GMSP. Copyright (C) 2015 John Wiley & Sons, Ltd.
C1 [Skiles, S. McKenzie; Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Belnap, Jayne] US Geol Survey, Southwest Biol Sci Ctr, Moab, UT USA.
[Holland, Lacey; Lin, John] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA.
[Reynolds, Richard L.; Goldstein, Harland L.] US Geol Survey, Geosci & Environm Change Sci Ctr, Denver, CO 80225 USA.
RP Skiles, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM skiles@jpl.nasa.gov
RI Painter, Thomas/B-7806-2016
FU NASA project [NNX10AO97G]; USGS Ecosystems and Climate and Land Use
programmes; NASA
FX We acknowledge Chris Landry/The Center for Snow and Avalanche Studies
for data retrieval, compilation, and availability. We would like to
thank three anonymous reviewers for their constructive comments, which
improved this manuscript. This work was funded by the NASA project
NNX10AO97G and JB received funding from the USGS Ecosystems and Climate
and Land Use programmes. Part of this work was performed at the Jet
Propulsion Laboratory, California Institute of Technology under a
contract from NASA. Any use of trade names is for descriptive purposes
only and does not imply endorsement by the U.S. Government.
NR 39
TC 8
Z9 8
U1 6
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD DEC 30
PY 2015
VL 29
IS 26
BP 5397
EP 5413
DI 10.1002/hyp.10569
PG 17
WC Water Resources
SC Water Resources
GA DB1OO
UT WOS:000368278100007
ER
PT J
AU Wimmer-Schweingruber, RF
Kohler, J
Hassler, DM
Guo, JN
Appel, JK
Zeitlin, C
Bohm, E
Ehresmann, B
Lohf, H
Bottcher, SI
Burmeister, S
Martin, C
Kharytonov, A
Brinza, DE
Posner, A
Reitz, G
Matthia, D
Rafkin, S
Weigle, G
Cucinotta, F
AF Wimmer-Schweingruber, Robert F.
Koehler, Jan
Hassler, Donald M.
Guo, Jingnan
Appel, Jan-Kristoffer
Zeitlin, Cary
Boehm, Eckart
Ehresmann, Bent
Lohf, Henning
Boettcher, Stephan I.
Burmeister, Soenke
Martin, Cesar
Kharytonov, Alexander
Brinza, David E.
Posner, Arik
Reitz, Guenther
Matthiae, Daniel
Rafkin, Scott
Weigle, Gerald
Cucinotta, Francis
TI On determining the zenith angle dependence of the Martian radiation
environment at Gale Crater altitudes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Space radiation environment; Gale Crater; Curiosity; Mars surface
radiation; MSL; zenith angle
ID TRIPLE COINCIDENCES; ASSESSMENT DETECTOR; VERTICAL DIRECTION;
COSMIC-RADIATION; ULTRA RADIATION; MAGNETIC-FIELD; MARS; STRATOSPHERE;
ANISOTROPY; MISSION
AB We report the zenith angle dependence of the radiation environment at Gale Crater on Mars. This is the first determination of this dependence on another planet than Earth and is important for future human exploration of Mars and understanding radiation effects in the Martian regolith. Within the narrow range of tilt angles (0 <= theta(0) <= 15 degrees) experienced by Curiosity on Mars, we find a dependence J proportional to cos(gamma)' (theta) with gamma' = 1.18 +/- 0.07, which is not too different from an isotropic radiation field and quite different from that at sea level on Earth where gamma' approximate to 2.0.
C1 [Wimmer-Schweingruber, Robert F.; Koehler, Jan; Guo, Jingnan; Appel, Jan-Kristoffer; Boehm, Eckart; Lohf, Henning; Boettcher, Stephan I.; Burmeister, Soenke; Martin, Cesar; Kharytonov, Alexander] Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany.
[Hassler, Donald M.; Ehresmann, Bent; Rafkin, Scott] Southwest Res Inst, Boulder, CO USA.
[Hassler, Donald M.] Paris XI Paris Sud, Inst Astrophys Spatiale, Orsay, Orsay, France.
[Zeitlin, Cary] Lockheed Martin IS & GS, Oakland, CA USA.
[Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Posner, Arik] NASA HQ, Washington, DC USA.
[Reitz, Guenther; Matthiae, Daniel] DLR, Inst Aerosp Med, Cologne, Germany.
[Weigle, Gerald] Big Head Endian, Burden, KS USA.
[Cucinotta, Francis] Dept Hlth Phys & Diagnost Serv, Las Vegas, NV USA.
RP Wimmer-Schweingruber, RF (reprint author), Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany.
EM wimmer@physik.uni-kiel.de
OI Matthia, Daniel/0000-0003-1507-0143
FU NASA (HEOMD) under JPL [1273039]; DLR's Space Administration grant
[50QM0501, 50 QM1201]; National Aeronautics and Space Administration
FX RAD is supported by NASA (HEOMD) under JPL subcontract 1273039 to
Southwest Research Institute and in Germany by DLR and DLR's Space
Administration grant 50QM0501 and 50 QM1201 to the Christian Albrechts
University, Kiel. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. In
particular, we would like to extend sincere gratitude to Jeff Simmonds,
Ashwin Vasavada, and Joy Crisp at JPL, Gale Allen, Michael Meyer, Chris
Moore, Victoria Friedensen at NASA HQ, and Heiner Witte at DLR in
Germany for their unwavering support of RAD over the years. This
research has made use of NASA's Astrophysics Data System. The data used
in this paper may be retrieved from the NASA Planetary Data System.
NR 17
TC 2
Z9 2
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2015
VL 42
IS 24
BP 10557
EP 10564
DI 10.1002/2015GL066664
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DC0WX
UT WOS:000368939700028
ER
PT J
AU Wanders, N
Wada, Y
AF Wanders, Niko
Wada, Yoshihide
TI Decadal predictability of river discharge with climate oscillations over
the 20th and early 21st century
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE discharge; climate oscillations; ENSO; PDO; NAO; AAO
ID WATER; RESOURCES
AB Long-term hydrological forecasts are important to increase our resilience and preparedness to extreme hydrological events. The skill in these forecasts is still limited due to large uncertainties inherent in hydrological models and poor predictability of long-term meteorological conditions. Here we show that strong (lagged) correlations exist between four different major climate oscillation modes and modeled and observed discharge anomalies over a 100year period. The strongest correlations are found between the El Nino-Southern Oscillation signal and river discharge anomalies all year round, while North Atlantic Oscillation and Antarctic Oscillation time series are strongly correlated with winter discharge anomalies. The correlation signal is significant for periods up to 5years for some regions, indicating a high added value of this information for long-term hydrological forecasting. The results suggest that long-term hydrological forecasting could be significantly improved by including the climate oscillation signals and thus improve our preparedness for hydrological extremes in the near future.
C1 [Wanders, Niko] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Wanders, Niko; Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands.
[Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Wanders, N (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
EM nwanders@princeton.edu
OI Wanders, Niko/0000-0002-7102-5454
FU NWO [GO-AO/30]; NWO Rubicon [825.15.003]; JSPS [2014-878]
FX NW is funded by NWO GO-AO/30 and NWO Rubicon 825.15.003, Y.W. is funded
by JSPS 2014-878. The authors would like to acknowledge Balazs Fekete
and Cedric H. David for reviewing the original manuscript and for their
constructive comments. The Princetonv3, GWSP3, WATCHv2, and WFDEI will
become available from the ISI-MIP2.1 archive. The hydrological model
PCR-GLOBWB is an open source hydrological model that can be obtained
from Utrecht University
(http://www.globalhydrology.nl/models/pcr-globwb-2-0/), and the
discharge observations are obtained from Global Runoff Data Centre
(http://www.bafg.de/GRDC/EN/Home/homepage_node. html).
NR 15
TC 3
Z9 3
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2015
VL 42
IS 24
BP 10689
EP 10695
DI 10.1002/2015GL066929
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DC0WX
UT WOS:000368939700048
ER
PT J
AU O'Reilly, CM
Sharma, S
Gray, DK
Hampton, SE
Read, JS
Rowley, RJ
Schneider, P
Lenters, JD
McIntyre, PB
Kraemer, BM
Weyhenmeyer, GA
Straile, D
Dong, B
Adrian, R
Allan, MG
Anneville, O
Arvola, L
Austin, J
Bailey, JL
Baron, JS
Brookes, JD
de Eyto, E
Dokulil, MT
Hamilton, DP
Havens, K
Hetherington, AL
Higgins, SN
Hook, S
Izmest'eva, LR
Joehnk, KD
Kangur, K
Kasprzak, P
Kumagai, M
Kuusisto, E
Leshkevich, G
Livingstone, DM
MacIntyre, S
May, L
Melack, JM
Mueller-Navarra, DC
Naumenko, M
Noges, P
Noges, T
North, RP
Plisnier, PD
Rigosi, A
Rimmer, A
Rogora, M
Rudstam, LG
Rusak, JA
Salmaso, N
Samal, NR
Schindler, DE
Schladow, SG
Schmid, M
Schmidt, SR
Silow, E
Soylu, ME
Teubner, K
Verburg, P
Voutilainen, A
Watkinson, A
Williamson, CE
Zhang, GQ
AF O'Reilly, Catherine M.
Sharma, Sapna
Gray, Derek K.
Hampton, Stephanie E.
Read, Jordan S.
Rowley, Rex J.
Schneider, Philipp
Lenters, John D.
McIntyre, Peter B.
Kraemer, Benjamin M.
Weyhenmeyer, Gesa A.
Straile, Dietmar
Dong, Bo
Adrian, Rita
Allan, Mathew G.
Anneville, Orlane
Arvola, Lauri
Austin, Jay
Bailey, John L.
Baron, Jill S.
Brookes, Justin D.
de Eyto, Elvira
Dokulil, Martin T.
Hamilton, David P.
Havens, Karl
Hetherington, Amy L.
Higgins, Scott N.
Hook, Simon
Izmest'eva, Lyubov R.
Joehnk, Klaus D.
Kangur, Kulli
Kasprzak, Peter
Kumagai, Michio
Kuusisto, Esko
Leshkevich, George
Livingstone, David M.
MacIntyre, Sally
May, Linda
Melack, John M.
Mueller-Navarra, Doerthe C.
Naumenko, Mikhail
Noges, Peeter
Noges, Tiina
North, Ryan P.
Plisnier, Pierre-Denis
Rigosi, Anna
Rimmer, Alon
Rogora, Michela
Rudstam, Lars G.
Rusak, James A.
Salmaso, Nico
Samal, Nihar R.
Schindler, Daniel E.
Schladow, S. Geoffrey
Schmid, Martin
Schmidt, Silke R.
Silow, Eugene
Soylu, M. Evren
Teubner, Katrin
Verburg, Piet
Voutilainen, Ari
Watkinson, Andrew
Williamson, Craig E.
Zhang, Guoqing
TI Rapid and highly variable warming of lake surface waters around the
globe
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE lakes; climate change; temperature
ID CLIMATE-CHANGE; AIR-TEMPERATURE; SPATIAL ASSOCIATION; REGRESSION TREES;
STATISTICS; TRENDS; MULTIPLE; BLOOMS
AB In this first worldwide synthesis of in situ and satellite-derived lake data, we find that lake summer surface water temperatures rose rapidly (global mean=0.34 degrees C decade(-1)) between 1985 and 2009. Our analyses show that surface water warming rates are dependent on combinations of climate and local characteristics, rather than just lake location, leading to the counterintuitive result that regional consistency in lake warming is the exception, rather than the rule. The most rapidly warming lakes are widely geographically distributed, and their warming is associated with interactions among different climatic factorsfrom seasonally ice-covered lakes in areas where temperature and solar radiation are increasing while cloud cover is diminishing (0.72 degrees C decade(-1)) to ice-free lakes experiencing increases in air temperature and solar radiation (0.53 degrees C decade(-1)). The pervasive and rapid warming observed here signals the urgent need to incorporate climate impacts into vulnerability assessments and adaptation efforts for lakes.
C1 [O'Reilly, Catherine M.; Rowley, Rex J.] Illinois State Univ, Dept Geog Geol, Normal, IL 61761 USA.
[Sharma, Sapna] York Univ, Dept Biol, Toronto, ON M3J 2R7, Canada.
[Gray, Derek K.] Calif Univ Pennsylvania, Dept Biol & Environm Sci, California, PA USA.
[Hampton, Stephanie E.] Washington State Univ, Ctr Environm Res Educ & Outreach, Pullman, WA 99164 USA.
[Read, Jordan S.] US Geol Survey, Ctr Integrated Data Analyt, Middleton, WI USA.
[Schneider, Philipp] Norwegian Inst Air Res, Kjeller, Norway.
[Lenters, John D.] LimnoTech, Ann Arbor, MI USA.
[McIntyre, Peter B.; Kraemer, Benjamin M.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA.
[Weyhenmeyer, Gesa A.] Uppsala Univ, Dept Ecol & Genet Limnol, Uppsala, Sweden.
[Straile, Dietmar] Univ Konstanz, Limnol Inst, Constance, Germany.
[Dong, Bo] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
[Adrian, Rita; Schmidt, Silke R.] Leibniz Inst Freshwater Ecol & Inland Fisheries, Dept Ecosyst Res, Berlin, Germany.
[Allan, Mathew G.] Univ Waikato, Environm Res Inst, Hamilton, New Zealand.
[Anneville, Orlane] Natl Inst Agr Res, UMR Ctr Alpin Rech Reseaux Troph Ecosyst Limn, Thonon Les Bains, France.
[Arvola, Lauri] Univ Helsinki, Lammi Biol Stn, Lammi, Finland.
[Austin, Jay] Univ Minnesota, Large Lakes Observ, Duluth, MN 55812 USA.
[Bailey, John L.] Laurentian Univ Sudbury, Cooperat Freshwater Ecol Unit, Minist Environm & Climate Change, Sudbury, ON, Canada.
[Baron, Jill S.] Colorado State Univ, Ft Collins Sci Ctr, US Geol Survey, Ft Collins, CO 80523 USA.
[Brookes, Justin D.; Rigosi, Anna] Univ Adelaide, Inst Environm, Sch Earth & Environm Sci, Water Res Ctr, Adelaide, SA, Australia.
[de Eyto, Elvira] Fisheries Ecosyst Advisory Serv, Inst Marine, Furnace, Newport, Ireland.
[Dokulil, Martin T.] Univ Innsbruck, Res Inst Limnol, Mondsee, Austria.
[Hamilton, David P.] Univ Waikato, Environm Res Inst, Hamilton, New Zealand.
[Havens, Karl] Univ Florida, 2Florida Sea Grant & UF IFAS, Gainesville, FL USA.
[Hetherington, Amy L.; Rudstam, Lars G.] Cornell Univ, Dept Nat Resources, Fernow Hall, Ithaca, NY 14853 USA.
[Higgins, Scott N.] Int Inst Sustainable Dev Expt Lakes Area, Winnipeg, MB, Canada.
[Hook, Simon] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
[Izmest'eva, Lyubov R.; Silow, Eugene] Irkutsk State Univ, Inst Biol, Irkutsk 664003, Russia.
[Joehnk, Klaus D.] CSIRO, Land & Water Flagship, Canberra, ACT, Australia.
[Kangur, Kulli] Estonian Univ Life Sci, Inst Agr & Environm Sci, Tartu, Estonia.
[Kasprzak, Peter] Leibniz Inst Freshwater Ecol & Inland Fisheries, Dept Expt Limnol, Berlin, Germany.
[Kumagai, Michio] Ritsumeikan Univ, Kusatsu, Japan.
[Kuusisto, Esko] Finnish Environm Inst, Helsinki, Finland.
[Leshkevich, George] NOAA, Great Lakes Environm Res Lab, 2205 Commonwealth Blvd, Ann Arbor, MI 48105 USA.
[Livingstone, David M.] Eawag Swiss Fed Inst Aquat Sci & Technol, Dept Water Resources & Drinking Water, Dubendorf, Switzerland.
[MacIntyre, Sally] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[May, Linda] Ctr Ecol & Hydrol, Bush Estate, Midlothian, Scotland.
[Melack, John M.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Mueller-Navarra, Doerthe C.] Univ Hamburg, Dept Biol, Hamburg, Germany.
[Naumenko, Mikhail] Russian Acad Sci, Limnol Inst, Hydrol Lab, St Petersburg 196140, Russia.
[Noges, Peeter; Noges, Tiina] Estonian Univ Life Sci, Inst Agr & Environm Sci, Ctr Limnol, Tartu, Estonia.
[North, Ryan P.] Helmholtz Zentrum Geesthacht, Inst Coastal Res, D-21502 Geesthacht, Germany.
[Plisnier, Pierre-Denis] Royal Museum Cent Africa, Dept Earth Sci, Tervuren, Belgium.
[Rimmer, Alon] Kinneret Limnol Lab, Israel Oceanog & Limnol Res, Migdal, Israel.
[Rogora, Michela] CNR, Inst Ecosyst Study, Verbania, Italy.
[Rusak, James A.] Ontario Minist Environm & Climate Change, Dorset Environm Sci Ctr, Dorset, ON, Canada.
[Salmaso, Nico] Ist Agr S Michele Adige Fdn E Mach, IASMA Res & Innovat Ctr, Trento, Trento, Italy.
[Samal, Nihar R.] Univ New Hampshire, Dept Nat Resources, Durham, NH 03824 USA.
[Samal, Nihar R.] Univ New Hampshire, Earth Syst Res Ctr, Durham, NH 03824 USA.
[Schindler, Daniel E.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.
[Schladow, S. Geoffrey] Univ Calif Davis, Dept Civil & Environm Engn, Tahoe Environm Res Ctr, Davis, CA 95616 USA.
[Schmid, Martin] Eawag Swiss Fed Inst Aquat Sci & Technol, Dept Surface Waters Res & Management, Kastanienbaum, Switzerland.
[Soylu, M. Evren] Meliksah Univ, Dept Civil Engn, Kayseri, Turkey.
[Teubner, Katrin] Univ Vienna, Fac Life Sci, Dept Limnol & Biol Oceanog, Vienna, Austria.
[Verburg, Piet] Natl Inst Water & Atmospher Res, Hamilton, New Zealand.
[Voutilainen, Ari] Univ Eastern Finland, Dept Biol, Kuopio, Finland.
[Watkinson, Andrew] Seqwater, Ipswich, Qld, Australia.
[Williamson, Craig E.] Miami Univ, Dept Biol, Oxford, OH 45056 USA.
[Zhang, Guoqing] Chinese Acad Sci, CAS Ctr Excellence Tibetan Plateau Earth Sci, Beijing, Peoples R China.
RP O'Reilly, CM (reprint author), Illinois State Univ, Dept Geog Geol, Normal, IL 61761 USA.
EM oreilly@ilstu.edu
RI Johnk, Klaus/B-3382-2008; Higgins, Scott/F-5700-2016; Silow,
Eugene/C-2958-2011; May, Linda/D-7943-2011; Baron, Jill/C-5270-2016;
Hook, Simon/D-5920-2016; ROGORA, MICHELA/B-9237-2008; Schmid,
Martin/C-3953-2009; Straile, Dietmar/A-4065-2008;
OI Johnk, Klaus/0000-0002-5972-4201; Silow, Eugene/0000-0002-7039-3220;
Baron, Jill/0000-0002-5902-6251; Hook, Simon/0000-0002-0953-6165;
ROGORA, MICHELA/0000-0003-3515-0220; Schmid, Martin/0000-0001-8699-5691;
Straile, Dietmar/0000-0002-7441-8552; Zhang,
Guoqing/0000-0003-2090-2813; Hampton, Stephanie/0000-0003-2389-4249
FU NASA Earth Science Division ROSES INCA; Science of Terra program; Aqua
program; NASA ROSES [E.2]; NSF [1147666, 1136637, 1030242, 1128040,
1204267]; USDA National Institute of Food and Agriculture Hatch
[0226747]; Estonian Ministry of Education and Research [IUT21-2];
University of Nebraska Institute of Agriculture and Natural Resources;
Inter-American Institute for Global Change Research [CRN3038]; German
Research Foundation DFG [STR 499/6-1]; Russian Ministry of Education and
Science research project [GR 01201461929]; Russian Science Foundation
[14-14-00400]; David and Lucille Packard Foundation
FX Data used in this study are available in Sharma et al. [2013]. Funding
in support of this work came from the following sources: NASA Earth
Science Division ROSES INCA and Science of Terra and Aqua programs and
NASA ROSES E.2; NSF awards 1147666, 1136637, 1030242, 1128040, and
1204267; USDA National Institute of Food and Agriculture Hatch 0226747;
Estonian Ministry of Education and Research IUT21-2; University of
Nebraska Institute of Agriculture and Natural Resources; Inter-American
Institute for Global Change Research CRN3038; German Research Foundation
DFG STR 499/6-1; Russian Ministry of Education and Science research
project GR 01201461929, Russian Science Foundation Project 14-14-00400;
and The David and Lucille Packard Foundation. We thank M. Moore and T.
Kratz for support in developing this initiative, N. Barabas and D.
Lofton for discussion, N. Keuler for help with statistical analyses, and
K. Woo for technical assistance. D. K. Gray, S.E. Hampton, C.M.
O'Reilly, and S. Sharma conceived the idea for this paper and co-led
this project. D. K. Gray, S.E. Hampton, B.M. Kraemer, P.B. McIntyre, C.
M. O'Reilly, J.S. Read, R.J. Rowley, S. Sharma, D. Straile, and G.A.
Weyhenmeyer conducted analyses incorporated into this paper. D. K. Gray,
B.M. Kraemer, C. M. O'Reilly, J. S. Read, R.J. Rowley, and S. Sharma
drafted figures, tables, and headings for this paper. B. Dong, D. K.
Gray, S.E. Hampton, B. M. Kraemer, P.B. McIntyre, C. M. O'Reilly, J. S.
Read, R.J. Rowley, P. Schneider, and S. Sharma wrote sections of the
text for this paper. All authors provided critical feedback, edits,
and/or commented on drafts of this paper. J. D. Brookes, D. P. Hamilton,
S. Hook, J. D. Lenters, D. Livingstone, P. B. McIntyre, C. M. O'Reilly,
J. S. Read, and P. Schneider played important roles in the early
development of the Global Lake Temperature Collaboration.
NR 49
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U1 35
U2 94
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2015
VL 42
IS 24
BP 10773
EP 10781
DI 10.1002/2015GL066235
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DC0WX
UT WOS:000368939700008
ER
PT J
AU Soibel, A
Rafol, SB
Khoshakhlagh, A
Nguyen, J
Hoglund, L
Fisher, AM
Keo, SA
Ting, DZY
Gunapala, SD
AF Soibel, Alexander
Rafol, Sir B.
Khoshakhlagh, Arezou
Jean Nguyen
Hoglund, Linda
Fisher, Anita M.
Keo, Sam. A.
Ting, David Z. -Y.
Gunapala, Sarath D.
TI Proton radiation effect on performance of InAs/GaSb complementary
barrier infrared detector
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID SUPERLATTICE; PHOTODIODES
AB In this work, we investigated the effect of proton irradiation on the performance of long wavelength infrared InAs/GaSb photodiodes (lambda(c) = 10.2 mu m), based on the complementary barrier infrared detector design. We found that irradiation with 68MeV protons causes a significant increase of the dark current from j(d) = 5 x 10(-5) A/cm(2) to j(d) = 6 x 10(-3) A/cm(2), at V-b = 0.1V, T = 80K and fluence 19.2 x 10(11) H+/cm(2). Analysis of the dark current as a function of temperature and bias showed that the dominant contributor to the dark current in these devices changes from diffusion current to tunneling current after proton irradiation. This change in the dark current mechanism can be attributed to the onset of surface leakage current, generated by trap-assisted tunneling processes in proton displacement damage areas located near the device sidewalls. (C) 2015 AIP Publishing LLC.
C1 [Soibel, Alexander; Rafol, Sir B.; Khoshakhlagh, Arezou; Jean Nguyen; Hoglund, Linda; Fisher, Anita M.; Keo, Sam. A.; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA.
RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91030 USA.
NR 29
TC 2
Z9 2
U1 0
U2 11
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD DEC 28
PY 2015
VL 107
IS 26
AR 261102
DI 10.1063/1.4938756
PG 4
WC Physics, Applied
SC Physics
GA DB3VY
UT WOS:000368442300002
ER
PT J
AU Arbabi, A
Briggs, RM
Horie, Y
Bagheri, M
Faraon, A
AF Arbabi, Amir
Briggs, Ryan M.
Horie, Yu
Bagheri, Mahmood
Faraon, Andrei
TI Efficient dielectric metasurface collimating lenses for mid-infrared
quantum cascade lasers
SO OPTICS EXPRESS
LA English
DT Article
ID HIGH-CONTRAST GRATINGS; ELEMENTS; FABRICATION; REFLECTORS; ANTENNA;
DESIGN
AB Light emitted from single-mode semiconductor lasers generally has large divergence angles, and high numerical aperture lenses are required for beam collimation. Visible and near infrared lasers are collimated using aspheric glass or plastic lenses, yet collimation of mid-infrared quantum cascade lasers typically requires more costly aspheric lenses made of germanium, chalcogenide compounds, or other infrared-transparent materials. Here we report mid-infrared dielectric metasurface flat lenses that efficiently collimate the output beam of single-mode quantum cascade lasers. The metasurface lenses are composed of amorphous silicon posts on a flat sapphire substrate and can be fabricated at low cost using a single step conventional UV binary lithography. Mid-infrared radiation from a 4.8 m m distributed-feedback quantum cascade laser is collimated using a polarization insensitive metasurface lens with 0.86 numerical aperture and 79% transmission efficiency. The collimated beam has a half divergence angle of 0.36 degrees and beam quality factor of M-2 = 1.02. (C) 2015 Optical Society of America
C1 [Arbabi, Amir; Horie, Yu; Faraon, Andrei] CALTECH, TJ Watson Lab Appl Phys, Pasadena, CA 91125 USA.
[Briggs, Ryan M.; Bagheri, Mahmood] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Faraon, A (reprint author), CALTECH, TJ Watson Lab Appl Phys, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM faraon@caltech.edu
FU Caltech/JPL Presidents and Directors Fund (PDF); NASA PICASSO program;
U.S. Department of Energy "LightMaterial Interactions in Energy
Conversion" Energy Frontier Research Center [DE-SC0001293]; Japan
Student Services Organization (JASSO) fellowship
FX This work was supported by the Caltech/JPL Presidents and Directors Fund
(PDF). R.M.B gratefully acknowledges support from the NASA PICASSO
program. Y.H. was supported as part of the U.S. Department of Energy
"LightMaterial Interactions in Energy Conversion" Energy Frontier
Research Center under grant DE-SC0001293 and a Japan Student Services
Organization (JASSO) fellowship. The device fabrication was performed in
the Kavli Nanoscience Institute at Caltech. The measurements were
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 30
TC 10
Z9 10
U1 7
U2 25
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 28
PY 2015
VL 23
IS 26
BP 33310
EP 33317
DI 10.1364/OE.23.033310
PG 8
WC Optics
SC Optics
GA DA7SO
UT WOS:000368004600042
PM 26831996
ER
PT J
AU Wright, MW
Morris, JF
Kovalik, JM
Andrews, KS
Abrahamson, MJ
Biswas, A
AF Wright, Malcolm W.
Morris, Jeffery F.
Kovalik, Joseph M.
Andrews, Kenneth S.
Abrahamson, Matthew J.
Biswas, Abhijit
TI Adaptive optics correction into single mode fiber for a low Earth
orbiting space to ground optical communication link using the OPALS
downlink
SO OPTICS EXPRESS
LA English
DT Article
AB An adaptive optics (AO) testbed was integrated to the Optical PAyload for Lasercomm Science (OPALS) ground station telescope at the Optical Communications Telescope Laboratory (OCTL) as part of the free space laser communications experiment with the flight system on board the International Space Station (ISS). Atmospheric turbulence induced aberrations on the optical downlink were adaptively corrected during an overflight of the ISS so that the transmitted laser signal could be efficiently coupled into a single mode fiber continuously. A stable output Strehl ratio of around 0.6 was demonstrated along with the recovery of a 50 Mbps encoded high definition (HD) video transmission from the ISS at the output of the single mode fiber. This proof of concept demonstration validates multi-Gbps optical downlinks from fast slewing low-Earth orbiting (LEO) spacecraft to ground assets in a manner that potentially allows seamless space to ground connectivity for future high data-rates network. (C) 2015 Optical Society of America
C1 [Wright, Malcolm W.; Kovalik, Joseph M.; Andrews, Kenneth S.; Abrahamson, Matthew J.; Biswas, Abhijit] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morris, Jeffery F.] Boeing Co, El Segundo, CA 90245 USA.
RP Wright, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM malcolm.wright@jpl.nasa.gov
NR 9
TC 5
Z9 5
U1 6
U2 15
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 28
PY 2015
VL 23
IS 26
BP 33705
EP 33712
DI 10.1364/OE.23.033705
PG 8
WC Optics
SC Optics
GA DA7SO
UT WOS:000368004600079
PM 26832033
ER
PT J
AU Verma, VB
Korzh, B
Bussieres, F
Horansky, RD
Dyer, SD
Lita, AE
Vayshenker, I
Marsili, F
Shaw, MD
Zbinden, H
Mirin, RP
Nam, SW
AF Verma, V. B.
Korzh, B.
Bussieres, F.
Horansky, R. D.
Dyer, S. D.
Lita, A. E.
Vayshenker, I.
Marsili, F.
Shaw, M. D.
Zbinden, H.
Mirin, R. P.
Nam, S. W.
TI High-efficiency superconducting nanowire single-photon detectors
fabricated from MoSi thin-films
SO OPTICS EXPRESS
LA English
DT Article
ID TIME
AB We report on MoSi SNSPDs which achieved high system detection efficiency (87.1 +/- 0.5% at 1542 nm) at 0.7 K and we demonstrate that these detectors can also be operated with saturated internal efficiency at a temperature of 2.3 K in a Gifford-McMahon cryocooler. We measured a minimum system jitter of 76 ps, maximum count rate approaching 10 MHz, and polarization dependence as low as 3.3 +/- 0.1%. The performance of MoSi SNSPDs at 2.3 K is similar to the performance of WSi SNSPDs at < 1 K. The higher operating temperature of MoSi SNSPDs makes these devices promising for widespread use due to the simpler and less expensive cryogenics required for their operation. (C) 2015 Optical Society of America
C1 [Verma, V. B.; Horansky, R. D.; Dyer, S. D.; Lita, A. E.; Vayshenker, I.; Mirin, R. P.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
[Korzh, B.; Bussieres, F.; Zbinden, H.] Univ Geneva, Grp Appl Phys, CH-1211 Geneva 4, Switzerland.
[Marsili, F.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Verma, VB (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA.
EM verma@nist.gov
RI Bussieres, Felix/E-5384-2011
OI Bussieres, Felix/0000-0003-0234-175X
FU DARPA InPho program; QUINESS program; Swiss NCCR Quantum Science in
Technology project
FX We acknowledge Claudio Barreiro for useful discussions, and the Swiss
Federal Institute of Metrology (METAS) for the calibration of the power
meters. NIST funding provided by the DARPA InPho and QUINESS programs.
Part of the work was funded by the Swiss NCCR Quantum Science in
Technology project.
NR 30
TC 13
Z9 13
U1 5
U2 22
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 28
PY 2015
VL 23
IS 26
BP 33792
EP 33801
DI 10.1364/OE.23.033792
PG 10
WC Optics
SC Optics
GA DA7SO
UT WOS:000368004600086
PM 26832040
ER
PT J
AU Sullivan, JT
Mcgee, TJ
Thompson, AM
Pierce, RB
Sumnicht, GK
Twigg, L
Eloranta, E
Hoff, RM
AF Sullivan, John T.
Mcgee, Thomas J.
Thompson, Anne M.
Pierce, R. Bradley
Sumnicht, Grant K.
Twigg, LaurenceW.
Eloranta, Edwin
Hoff, Raymond M.
TI Characterizing the lifetime and occurrence of stratospheric-tropospheric
exchange events in the rockymountain region using high-resolution ozone
measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POTENTIAL VORTICITY; NORTHERN-HEMISPHERE; LOW SYSTEMS; TROPOPAUSE;
CLIMATOLOGY; LIDAR; INTRUSIONS; TRANSPORT; EUROPE; IMPACT
AB The evolution of a Stratospheric-Tropospheric Exchange (STE) event from 4 to 8 August 2014 at Fort Collins, Colorado, is described. The event is characterized with observations from the Goddard Space Flight Center TROPospheric OZone (TROPOZ) Differential Absorption Lidar, the University of Wisconsin High Spectral Resolution Lidar, and multiple ozonesondes during NASA's Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality and the Front Range Air Pollution and Photochemistry Experiment (FRAPPE) campaigns. Based on the extended TROPOZ observations throughout the entire campaign, it was found that STE events have largely contributed to an additional 10-30 ppbv of ozone at Fort Collins. Additional measurements of ozone and relative humidity from the Atmospheric Infrared Sounder are characterize the transport of the intrusion. The Real-time Air Quality Modeling System simulated ozone agrees well with the TROPOZ ozone concentrations and altitude during the STE event. To extend the analysis into other seasons and years, the modeled ozone to potential vorticity ratio is used as a tracer for stratospheric air residing below the tropopause. It is found that at Fort Collins, CO, and depending on season from 2012 to 2014, between 18 and 31% of tropospheric ozone corresponds to stratospheric air. A relationship to determine the lifetime of stratospheric air below the tropopause is derived using the simulated ratio tracer. Results indicate that throughout summer 2014, 43% of stratospheric air resided below the tropopause for less than 12 h. However, nearly 39% persisted below the tropopause for 12-48 h and likely penetrated deeper in the troposphere.
C1 [Sullivan, John T.; Mcgee, Thomas J.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Sullivan, John T.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA.
[Pierce, R. Bradley] NOAA NESDIS Ctr Satellite Applicat & Res Cooperat, Adv Satellite Prod Branch, Ctr Satellite Applicat & Res, Madison, WI USA.
[Sumnicht, Grant K.; Twigg, LaurenceW.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Eloranta, Edwin] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Hoff, Raymond M.] Univ Maryland Baltimore Cty, Dept Atmospher Sci, Baltimore, MD 21228 USA.
[Hoff, Raymond M.] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
RP Sullivan, JT (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
EM john.t.sullivan@nasa.gov
RI Pierce, Robert Bradley/F-5609-2010; Thompson, Anne /C-3649-2014
OI Pierce, Robert Bradley/0000-0002-2767-1643; Thompson, Anne
/0000-0002-7829-0920
FU UMBC/JCE [8306, 374]; Maryland Department of the Environment (MDE)
[U00P4400079]; NOAA-CREST CCNY Foundation [49173B-02]; National
Aeronautics and Space Administration; NASA DISCOVER AQ grant [NNX10ARG];
Colorado Department of Public Health and Environment (CDPHE); NASA
Postdoctoral Program; NASA HQ; NASA Tropospheric Chemistry Program;
Tropospheric Ozone Lidar Network (TOLNet); Pennsylvania State University
FX Unless otherwise noted, all data used in this study can be found in the
DISCOVER-AQ/FRAPPE data archive
(http://www-air.larc.nasa.gov/missions/discover-aq), the TOLNet data
archive (http://www-air.larc.nasa.gov/missions/TOLNet), or the RAQMS
data archive (http://raqms.ssec.wisc.edu). This work was supported by
UMBC/JCET (Task 374, Project 8306), the Maryland Department of the
Environment (MDE, contract U00P4400079), NOAA-CREST CCNY Foundation
(subcontract 49173B-02), and the National Aeronautics and Space
Administration. The Platteville Nittany Atmospheric Trailer and
Integrated Validation Experiment (NATIVE) operations were sponsored by
NASA DISCOVER AQ grant NNX10ARG and the Pennsylvania State University.
The University of Wisconsin HSRL operations were supported from the
Colorado Department of Public Health and Environment (CDPHE). This
research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center. The authors gratefully
acknowledge support provided by NASA HQ, the NASA Tropospheric Chemistry
Program, and the Tropospheric Ozone Lidar Network (TOLNet). Thanks to
the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT
transport and dispersion model and thanks to the Cooperative Institute
for Mesoscale Meteorological Studies (CIMMS) for supporting the RAQMS
model runs. Thanks to the helpfulness and expertise of Ryan Stauffer,
Hannah Halliday, and Nikolai Balashov who worked with the NATIVE trailer
at Platteville. Thanks to Debra Wicks Kollonige for providing her
insight and recommendations on this work. Also, thanks to A.O. Langford
for the extensive discussions on the heritage of stratospheric events.
The views, opinions, and findings contained in this report are those of
the author(s) and should not be construed as an official National
Oceanic and Atmospheric Administration or U.S. Government position,
policy, or decision.
NR 40
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U1 5
U2 15
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 DEC 27
PY 2015
VL 120
IS 24
BP 12410
EP 12424
DI 10.1002/2015JD023877
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TU
UT WOS:000369846700006
ER
PT J
AU Kim, YH
Kim, MK
Lau, WKM
Kim, KM
Cho, CH
AF Kim, Yeon-Hee
Kim, Maeng-Ki
Lau, William K. M.
Kim, Kyu-Myong
Cho, Chun-Ho
TI Possible mechanism of abrupt jump in winter surface air temperature in
the late 1980s over the Northern Hemisphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC CIRCULATION; REGIME SHIFTS; ALEUTIAN LOW; REANALYSIS;
EXPANSION; DECREASE; MONSOON; INDEX; SEA
AB Possible cause of an abrupt warming in winter mean surface air temperature in the midlatitudes of the Northern Hemisphere in the late 1980s is investigated using observation and reanalysis data. To determine the timing of abrupt warming, we use a regime shift index based on detection of the largest significant differences between the mean values of two contiguous periods. Results show that the abrupt warming occurred in association with a regime shift after the 1980's in which the zonal mean sea level pressure (SLP) is significantly increased (decreased) at the latitude 25-35 degrees N (60-70 degrees N), in the form of north-south dipole-like SLP anomaly spanning the subtropics and high latitude. The dipole SLP anomaly can be attributed to a northward expansion of Hadley cell, a poleward broadening and intensification of the Ferrel cell, coupled with a collapse of polar cell. During the abrupt warming, strong anomalous southerly warm advection at the surface was induced by an enhanced and expanded Ferrel circulation, in association with a northward and downward shift of maximum center of northward eddy heat flux over the midlatitudes. An intensification of polar jet subsequent to regime shift may be instrumental in sustaining the warming up to more than 5 years.
C1 [Kim, Yeon-Hee] Pohang Univ Sci & Technol, Sch Environm Sci & Engn, Pohang, South Korea.
[Kim, Maeng-Ki] Kongju Natl Univ, Dept Atmospher Sci, Gongju, South Korea.
[Lau, William K. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kim, Kyu-Myong] NASA, Goddard Space Flight Ctr, Lab Atmospheres, Greenbelt, MD USA.
[Cho, Chun-Ho] Natl Inst Meteorol Sci, Seogwipo, South Korea.
RP Kim, MK (reprint author), Kongju Natl Univ, Dept Atmospher Sci, Gongju, South Korea.
EM mkkim@kongju.ac.kr
RI Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Strategic Science Investment fund at NASA Goddard Space Flight Center;
Modeling Analysis and Prediction program of NASA Headquarters; DOE/PNNL
[4331620]; Development and application of methodology for climate change
prediction [NIMR-2012-B-2]
FX The authors thank the Physical Science Division (PSD) for providing the
NCEP Reanalysis I data from their website http://www.esrl.noaa.gov/psd/,
Sergei N. Rodionov for providing RSI tool from the website
http://www.climatelogic.com/home,and the Climate Research Unit (CRU) for
providing global land surface monthly temperature data from the website
www.cru.uea.ac.uk/data. This research is supported by a project
"NIMR-2012-B-2 (Development and application of methodology for climate
change prediction)". This work was partially supported by the Strategic
Science Investment fund at NASA Goddard Space Flight Center and the
Modeling Analysis and Prediction program of NASA Headquarters. Partial
support was also provided by the DOE/PNNL grant 4331620 to ESSIC,
University of Maryland.
NR 32
TC 0
Z9 1
U1 5
U2 8
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 DEC 27
PY 2015
VL 120
IS 24
BP 12474
EP 12485
DI 10.1002/2015JD023864
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TU
UT WOS:000369846700010
PM 27818850
ER
PT J
AU Guan, B
Waliser, DE
AF Guan, Bin
Waliser, Duane E.
TI Detection of atmospheric rivers: Evaluation and application of an
algorithm for global studies
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; WESTERN UNITED-STATES; EXTREME PRECIPITATION;
GEOPOTENTIAL HEIGHT; INLAND PENETRATION; PACIFIC-OCEAN; CALIFORNIA;
RAINFALL; IMPACTS; SEASON
AB Atmospheric rivers (ARs) are narrow, elongated, synoptic jets of water vapor that play important roles in the global water cycle and regional weather/hydrology. A technique is developed for objective detection of ARs on the global domain based on characteristics of the integrated water vapor transport (IVT). AR detection involves thresholding 6-hourly fields of ERA-Interim IVT based on the 85th percentile specific to each season and grid cell and a fixed lower limit of 100 kg m(-1) s(-1) and checking for the geometry requirements of length > 2000 km, length/width ratio > 2, and other considerations indicative of AR conditions. Output of the detection includes the AR shape, axis, landfall location, and basic statistics of each detected AR. The performance of the technique is evaluated by comparison to AR detection in the western North America, Britain, and East Antarctica with three independently conducted studies using different techniques, with over similar to 90% agreement in AR dates. Among the parameters tested, AR detection shows the largest sensitivity to the length criterion in terms of changes in the resulting statistical distribution of AR intensity and geometry. Global distributions of key AR characteristics are examined, and the results highlight the global footprints of ARs and their potential importance on global and regional scales. Also examined are seasonal dependence of AR frequency and precipitation and their modulation by four prominent modes of large-scale climate variability. The results are in broad consistency with previous studies that focused on landfalling ARs in the west coasts of North America and Europe.
C1 [Guan, Bin; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Guan, Bin; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Guan, B (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
EM bin.guan@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
FU NSF [AGS-1221013]; NASA Energy and Water cycle Study (NEWS) program
FX This research was supported by NSF AGS-1221013 and the NASA Energy and
Water cycle Study (NEWS) program. The IWV-based AR landfall record was
prepared and provided by Paul Neiman of the NOAA Earth System Research
Laboratory and gratefully acknowledged. Comments and suggestions by
Jinwon Kim of UCLA and Marty Ralph of UCSD/Scripps Institution of
Oceanography were helpful and appreciated. This research was in part
carried out on behalf of the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 56
TC 10
Z9 10
U1 8
U2 17
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 DEC 27
PY 2015
VL 120
IS 24
BP 12514
EP 12535
DI 10.1002/2015JD024257
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TU
UT WOS:000369846700013
ER
PT J
AU Taylor, PC
Kato, S
Xu, KM
Cai, M
AF Taylor, Patrick C.
Kato, Seiji
Xu, Kuan-Man
Cai, Ming
TI Covariance between Arctic sea ice and clouds within atmospheric state
regimes at the satellite footprint level
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MIXED-PHASE STRATOCUMULUS; INVERSION STRENGTH; CLIMATE MODELS; SURFACE;
FLUXES; OCEAN; AMPLIFICATION; MOISTURE; SYSTEM; ALBEDO
AB Understanding the cloud response to sea ice change is necessary for modeling Arctic climate. Previous work has primarily addressed this problem from the interannual variability perspective. This paper provides a refined perspective of sea ice-cloud relationship in the Arctic using a satellite footprint-level quantification of the covariance between sea ice and Arctic low cloud properties from NASA A-Train active remote sensing data. The covariances between Arctic low cloud properties and sea ice concentration are quantified by first partitioning each footprint into four atmospheric regimes defined using thresholds of lower tropospheric stability and midtropospheric vertical velocity. Significant regional variability in the cloud properties is found within the atmospheric regimes indicating that the regimes do not completely account for the influence of meteorology. Regional anomalies are used to account for the remaining meteorological influence on clouds. After accounting for meteorological regime and regional influences, a statistically significant but weak covariance between cloud properties and sea ice is found in each season for at least one atmospheric regime. Smaller average cloud fraction and liquid water are found within footprints with more sea ice. The largest-magnitude cloud-sea ice covariance occurs between 500m and 1.2 km when the lower tropospheric stability is between 16 and 24 K. The covariance between low cloud properties and sea ice is found to be largest in fall and is accompanied by significant changes in boundary layer temperature structure where larger average near-surface static stability is found at larger sea ice concentrations.
C1 [Taylor, Patrick C.; Kato, Seiji; Xu, Kuan-Man] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA.
[Cai, Ming] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
RP Taylor, PC (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA.
EM patrick.c.taylor@nasa.gov
RI Xu, Kuan-Man/B-7557-2013; Taylor, Patrick/D-8696-2015
OI Xu, Kuan-Man/0000-0001-7851-2629; Taylor, Patrick/0000-0002-8098-8447
FU NASA Interdisciplinary Studies Program [NNH12ZDA001N-IDS]; NASA Energy
and Water Cycle Studies program
FX The authors would like to thank the three anonymous reviewers of this
manuscript for their insightful comments significantly improving this
manuscript. This work is funded by the NASA Interdisciplinary Studies
Program grant NNH12ZDA001N-IDS. The processing of the C3M data used in
this analysis was funded under the NASA Energy and Water Cycle Studies
program and is available from the Langley Atmospheric Science Data
Center (http://eosweb.larc.nasa.gov).
NR 67
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U1 1
U2 10
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 DEC 27
PY 2015
VL 120
IS 24
BP 12656
EP 12678
DI 10.1002/2015JD023520
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TU
UT WOS:000369846700021
PM 27818851
ER
PT J
AU Smith, AK
Lopez-Puertas, M
Xu, JY
Mlynczak, MG
AF Smith, Anne K.
Lopez-Puertas, Manuel
Xu, Jiyao
Mlynczak, Martin G.
TI The heating efficiency of the exothermic reaction H + O-3 in the
mesosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATOMIC OXYGEN; MESOPAUSE REGION; CHEMISTRY; MESOSPHERE; ALGORITHM
AB An important source of heating in the mesosphere is the exothermic reaction of ozone with atomic hydrogen, which generates hydroxyl in a vibrationally excited state. Some of the energy from the excited states is lost through emissions in the Meinel bands. The heating efficiency of the exothermic reaction is therefore less than one. In this study, we incorporate a model of the vibrationally excited OH into the Whole Atmosphere Community Climate Model in order to calculate the heating efficiency of this reaction interactively with the model chemistry and dynamics. The global annual mean efficiency is near 60%, but the value can differ by 20% or more depending on altitude and season. A formula for accurately including the dependence of efficiency on atomic oxygen, temperature, and pressure is given.
C1 [Smith, Anne K.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Lopez-Puertas, Manuel] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Xu, Jiyao] Chinese Acad Sci, Beijing, Peoples R China.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Smith, AK (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM aksmith@ucar.edu
OI Lopez-Puertas, Manuel/0000-0003-2941-7734
FU National Science Foundation; National Science Foundation (NSF); Office
of Science of the U.S. Department of Energy; Spanish MINECO
[AYA2011-23552]; EC FEDER funds
FX The National Center for Atmospheric Research (NCAR) is sponsored by the
National Science Foundation. WACCM is a component of the Community Earth
System Model (CESM), which is supported by the National Science
Foundation (NSF) and the Office of Science of the U.S. Department of
Energy. CESM and the files needed to run it are available from NCAR; see
https://www2.cesm.ucar.edu/models/current. The modified routines used in
this paper and the results of the model simulations are available from
the lead author. Computing resources were provided by NCAR's
Computational and Information Systems Laboratory (CISL). M. L.-P. has
been supported by the Spanish MINECO under grant AYA2011-23552 and EC
FEDER funds. We thank D.R. Marsh and S.C. Solomon for their comments and
discussion.
NR 24
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U1 1
U2 6
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 DEC 27
PY 2015
VL 120
IS 24
BP 12739
EP 12747
DI 10.1002/2015JD024061
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DD3TU
UT WOS:000369846700026
ER
PT J
AU Stolzenburg, F
Johnson, MT
Lee, KN
Jacobson, NS
Faber, KT
AF Stolzenburg, F.
Johnson, M. T.
Lee, K. N.
Jacobson, N. S.
Faber, K. T.
TI The interaction of calcium-magnesium-aluminosilicate with ytterbium
silicate environmental barrier materials
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE Environmental barrier coating; Ceramic; CMAS; X-ray diffraction;
Energy-dispersive X-ray spectroscopy
ID TURBINE BLADE; WATER-VAPOR; COATINGS; CMAS; DEGRADATION; TEMPERATURE;
CERAMICS; DEPOSITS; VOLATILITY; RECESSION
AB The interactions of two potential topcoat materials for environmental barrier coatings, Yb2SiO5 and Yb2Si2O7, with calcium-magnesium-aluminosilicate (CMAS) engine deposits were studied. X-ray diffraction, scanning electron microscopy, energy-dispersive X-ray spectroscopy, and electron diffraction were used to investigate the phase transformation associated with the exposure of Yb2SiO5 and Yb2Si2O7 to CMAS at 1300 degrees C. It was found that Yb2SiO5 strongly reacts with CMAS to completely dissolve the Yb2SiO5 and form hexagonal Ca2Yb8(SiO4)(6)O-2 deposits. In contrast, no discernable reaction between CMAS and Yb2Si2O7, was observed over the 96-h exposure. (C)2015 Elsevier B.V. All rights reserved.
C1 [Stolzenburg, F.; Faber, K. T.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Johnson, M. T.; Faber, K. T.] CALTECH, Pasadena, CA 91125 USA.
[Lee, K. N.] Rolls Royce Corp, Mat Engn, Indianapolis, IN 46241 USA.
[Jacobson, N. S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Faber, KT (reprint author), CALTECH, MC 138-78, Pasadena, CA 91125 USA.
EM ktfaber@caltech.edu
FU DOE Office of Science by Argonne National Laboratory
[DE-AC02-06CH11357]; MRSEC program of the National Science Foundation at
the Materials Research Center of Northwestern University [DMR-1121262];
NSF-NSEC; NSF-MRSEC; Keck Foundation; State of Illinois; Northwestern
University
FX This research was made possible by the Advanced Photon Source, a U.S.
Department of Energy (DOE) Office of Science User Facility operated for
the DOE Office of Science by Argonne National Laboratory under Contract
No. DE-AC02-06CH11357. This work made use of the OMM Facility supported
by the MRSEC program of the National Science Foundation (DMR-1121262) at
the Materials Research Center of Northwestern University. SEM and
FIB-SEM (FEI) were performed in the EPIC facility of NUANCE Center at
Northwestern University. NUANCE Center is supported by NSF-NSEC,
NSF-MRSEC, Keck Foundation, the State of Illinois, and Northwestern
University. X-ray diffraction experiments were performed at the Cohen
X-ray Lab at Northwestern University. The Cohen X-ray Facility is
supported by NSF-MRSEC. A Northwestern University Terminal Year
Fellowship provided partial support for F.S.
NR 29
TC 2
Z9 2
U1 2
U2 19
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD DEC 25
PY 2015
VL 284
BP 44
EP 50
DI 10.1016/j.surfcoat.2015.08.069
PG 7
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA DA5RH
UT WOS:000367859700008
ER
PT J
AU Appleby, MP
Zhu, DM
Morscher, GN
AF Appleby, M. P.
Zhu, Dongming
Morscher, G. N.
TI Mechanical properties and real-time damage evaluations of environmental
barrier coated SiC/SiC CMCs subjected to tensile loading under thermal
gradients
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE Environmental barrier coating; Ceramic matrix composite; Electrical
resistance; Acoustic emission; Digital image correlation
ID SIO2 SCALE VOLATILITY; MATRIX COMPOSITES; COMBUSTION CONDITIONS;
ACOUSTIC-EMISSION; RECESSION; COATINGS; ACCUMULATION; TEMPERATURE;
DESIGN; MODEL
AB Environmental barrier coating (EBC) coated ceramic matrix composite (CMC) systems are currently being investigated for use as turbine engine hot-section components in extreme environments. In these extreme conditions, it becomes critical to understand material response to environmental exposure and performance under thermo-mechanical loading. Electrical resistance (ER) monitoring has recently been correlated to tensile damage accumulation in SiC/SiC CMCs, and the focus of this study is to extend the use of ER to evaluate high-temperature thermal gradient fracture of EBC/CMC systems. Tensile strength tests were performed at high temperature (1200 degrees C) using a laser-based heat-flux technique. Specimens included an as-produced SiC/SiC CMC and coated SiC/SiC substrate that have been exposed to simulated combustion environments in a high-pressure burner rig. Localized stress-dependent damage was determined using acoustic emission (AE) monitoring and compared to full-field strain mapping using a high-temperature digital image correlation (DIC) technique. The results are compared with in-situ ER monitoring, and post-test inspection of the samples in order to correlate ER response to damage evolution. Published by Elsevier B.V.
C1 [Appleby, M. P.; Zhu, Dongming] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Appleby, M. P.; Morscher, G. N.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
RP Appleby, MP (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
FU NASA Glenn Research Center, Transformational Tools and Technologies
Project
FX This work was supported by the NASA Glenn Research Center,
Transformational Tools and Technologies Project. The authors would like
to gratefully acknowledge Ron Phillips and Nathan Wilmoth of NASA GRC
for their mechanical testing and technical support.
NR 34
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U1 11
U2 39
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD DEC 25
PY 2015
VL 284
BP 318
EP 326
DI 10.1016/j.surfcoat.2015.07.042
PG 9
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA DA5RH
UT WOS:000367859700047
ER
PT J
AU Qin, J
Yanovsky, I
Yin, WT
AF Qin, Jing
Yanovsky, Igor
Yin, Wotao
TI Efficient simultaneous image deconvolution and upsampling algorithm for
low-resolution microwave sounder data
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE nonlinear image processing; deconvolution; resolution; microwaves;
upsampling; advanced microwave sounding unit; microwave humidity
sounder; alternating direction method of multipliers
ID RECONSTRUCTION
AB Microwave imaging has been widely used in the prediction and tracking of hurricanes, typhoons, and tropical storms. Due to the limitations of sensors, the acquired remote sensing data are usually blurry and have relatively low resolution, which calls for the development of fast algorithms for deblurring and enhancing the resolution. We propose an efficient algorithm for simultaneous image deconvolution and upsampling for low-resolution microwave hurricane data. Our model involves convolution, downsampling, and the total variation regularization. After reformulating the model, we are able to apply the alternating direction method of multipliers and obtain three subproblems, each of which has a closed-form solution. We also extend the framework to the multichannel case with the multichannel total variation regularization. A variety of numerical experiments on synthetic and real Advanced Microwave Sounding Unit and Microwave Humidity Sounder data were conducted. The results demonstrate the outstanding performance of the proposed method. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Qin, Jing; Yin, Wotao] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA.
[Yanovsky, Igor] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yanovsky, Igor] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
RP Qin, J (reprint author), Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA.
EM jxq@ucla.edu
OI Qin, Jing/0000-0001-8630-2904
FU National Aeronautics and Space Administration; NSF [DMS-1217239,
DMS-1317602, ECCS-1462398]
FX The research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. I. Yanovsky acknowledges the
support from NSF Grant No. DMS-1217239. W. Yin acknowledges the support
from NSF Grant No. DMS-1317602 and ECCS-1462398.
NR 24
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U1 1
U2 1
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD DEC 24
PY 2015
VL 9
AR 095035
DI 10.1117/1.JRS.9.095035
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DE5KL
UT WOS:000370669800001
ER
PT J
AU Chen, XM
Zhang, LY
Park, C
Fay, CC
Wang, XQ
Ke, CH
AF Chen, Xiaoming
Zhang, Liuyang
Park, Cheol
Fay, Catharine C.
Wang, Xianqiao
Ke, Changhong
TI Mechanical strength of boron nitride nanotube-polymer interfaces
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATION; CARBON NANOTUBES; ELASTIC-MODULUS; EPOXY;
COMPOSITES; TESTS; FIELD
AB We investigate the mechanical strength of boron nitride nanotube (BNNT) polymer interfaces by using in situ electron microscopy nanomechanical single-tube pull-out techniques. The nanomechanical measurements show that the shear strengths of BNNT-epoxy and BNNT-poly(methyl methacrylate) interfaces reach 323 and 219 MPa, respectively. Molecular dynamics simulations reveal that the superior load transfer capacity of BNNT-polymer interfaces is ascribed to both the strong van der Waals interactions and Coulomb interactions on BNNT-polymer interfaces. The findings of the extraordinary mechanical strength of BNNT-polymer interfaces suggest that BNNTs are excellent reinforcing nanofiller materials for light-weight and high-strength polymer nanocomposites. (C) 2015 AIP Publishing LLC.
C1 [Zhang, Liuyang; Wang, Xianqiao] Univ Georgia, Coll Engn, Athens, GA 30602 USA.
[Chen, Xiaoming; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
[Park, Cheol; Fay, Catharine C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
RP Wang, XQ (reprint author), Univ Georgia, Coll Engn, Athens, GA 30602 USA.
EM xqwang@uga.edu; cke@binghamton.edu
RI Ke, Changhong/C-4064-2008; Zhang, Liuyang/C-2987-2017
OI Zhang, Liuyang/0000-0001-7170-5452
FU U.S. Air Force Office of Scientific Research-Low Density Materials
Program [FA9550-11-1-0042, FA9550-10-1-0451, FA9550-15-1-0491]; NSF MRI
[CMMI-1429176]
FX This work was funded by U.S. Air Force Office of Scientific Research-Low
Density Materials Program under Grant Nos. FA9550-11-1-0042,
FA9550-10-1-0451, and FA9550-15-1-0491. The Raman measurements were
performed using a facility that was supported by an NSF MRI Award (No.
CMMI-1429176). The simulations were performed at the Georgia Advanced
Computing Resource Center at the University of Georgia.
NR 42
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U2 29
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD DEC 21
PY 2015
VL 107
IS 25
AR 253105
DI 10.1063/1.4936755
PG 5
WC Physics, Applied
SC Physics
GA DB3VW
UT WOS:000368442100037
ER
PT J
AU Cho, JYK
Polichtchouk, I
Thrastarson, HT
AF Cho, J. Y. -K.
Polichtchouk, I.
Thrastarson, H. Th.
TI Sensitivity and variability redux in hot-Jupiter flow simulations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; waves; turbulence; methods: numerical; planets and
satellites: atmospheres
ID GENERAL-CIRCULATION MODELS; EXTRASOLAR GIANT PLANETS; ATMOSPHERIC
CIRCULATION; HD 209458B; GRAVITY-WAVES; INSTABILITY; 189733B
AB We revisit the issues of sensitivity to initial flow and intrinsic variability in hot-Jupiter atmospheric flow simulations, issues originally investigated by Cho et al. and Thrastarson & Cho. The flow in the lower region (similar to 1 to 20 MPa) 'dragged' to immobility and uniform temperature on a very short time-scale, as in Liu & Showman, leads to effectively a complete cessation of variability as well as sensitivity in three-dimensional (3D) simulations with traditional primitive equations. Such momentum (Rayleigh) and thermal (Newtonian) drags are, however, ad hoc for 3D giant planet simulations. For 3D hot-Jupiter simulations, which typically already employ a strong Newtonian drag in the upper region, sensitivity is not quenched if only the Newtonian drag is applied in the lower region, without the strong Rayleigh drag: in general, both sensitivity and variability persist if the two drags are not applied concurrently in the lower region. However, even when the drags are applied concurrently, vertically propagating planetary waves give rise to significant variability in the similar to 0.05-0.5 MPa region, if the vertical resolution of the lower region is increased (e.g. here with 1000 layers for the entire domain). New observations on the effects of the physical setup and model convergence in 'deep' atmosphere simulations are also presented.
C1 [Cho, J. Y. -K.; Polichtchouk, I.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
[Cho, J. Y. -K.] Harvard Univ, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Polichtchouk, I.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Thrastarson, H. Th.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cho, JYK (reprint author), Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
EM J.Cho@qmul.ac.uk
FU UK's Science and Technology Facilities Council; NASA
FX The authors acknowledge helpful discussions with Craig Agnor, Tommi
Koskinen and Stephen Thomson - and particularly for their careful
reading of the manuscript. The authors also acknowledge the hospitality
of the Kavli Institute for Theoretical Physics, Santa Barbara, where
some of this work was completed. IP is supported by UK's Science and
Technology Facilities Council research studentship. HThT is supported by
the NASA Post-doctoral Program at the Jet Propulsion Laboratory,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 33
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 DEC 21
PY 2015
VL 454
IS 4
BP 3423
EP 3431
DI 10.1093/mnras/stv1947
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600006
ER
PT J
AU Rampino, MR
Caldeira, K
AF Rampino, Michael R.
Caldeira, Ken
TI Periodic impact cratering and extinction events over the last 260
million years
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE comets: general; Earth; meteorites meteors meteoroids; planets and
satellites: surfaces
ID TIME-SERIES ANALYSIS; MASS EXTINCTIONS; FOSSIL RECORD; DARK-MATTER; OORT
CLOUD; BIODIVERSITY; CYCLES; TESTS; EARTH; HYPOTHESIS
AB The claims of periodicity in impact cratering and biological extinction events are controversial. A newly revised record of dated impact craters has been analyzed for periodicity, and compared with the record of extinctions over the past 260 Myr. A digital circular spectral analysis of 37 crater ages (ranging in age from 15 to 254 Myr ago) yielded evidence for a significant 25.8 +/- 0.6 Myr cycle. Using the same method, we found a significant 27.0 +/- 0.7 Myr cycle in the dates of the eight recognized marine extinction events over the same period. The cycles detected in impacts and extinctions have a similar phase. The impact crater dataset shows 11 apparent peaks in the last 260 Myr, at least 5 of which correlate closely with significant extinction peaks. These results suggest that the hypothesis of periodic impacts and extinction events is still viable.
C1 [Rampino, Michael R.] NYU, Dept Biol, New York, NY 10003 USA.
[Rampino, Michael R.] NYU, Dept Environm Studies, New York, NY 10003 USA.
[Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Caldeira, Ken] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
RP Rampino, MR (reprint author), NYU, Dept Biol, New York, NY 10003 USA.
EM mrr1@nyu.edu
RI Caldeira, Ken/E-7914-2011
FU NYU
FX We thank T. Volk for helpful discussions and L. Jetsu for comments. J.
Deutscher drafted Fig. 2. An NYU Research Challenge Fund grant provided
support.
NR 50
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U1 5
U2 16
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 DEC 21
PY 2015
VL 454
IS 4
BP 3480
EP 3484
DI 10.1093/mnras/stv2088
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600011
ER
PT J
AU Keek, L
Cumming, A
Wolf, Z
Ballantyne, DR
Suleimanov, VF
Kuulkers, E
Strohmayer, TE
AF Keek, L.
Cumming, A.
Wolf, Z.
Ballantyne, D. R.
Suleimanov, V. F.
Kuulkers, E.
Strohmayer, T. E.
TI The imprint of carbon combustion on a superburst from the accreting
neutron star 4U 1636-536
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: 4U 1636-536; stars:
neutron; X-rays: binaries; X-rays: bursts
ID RAY-TIMING-EXPLORER; ELECTRON-ION PLASMAS; ANGULAR-DISTRIBUTION; MODELS;
DISK; EMISSION; EVOLUTION; EQUATION; BURSTS; REFLECTION
AB Superbursts are hours-long X-ray flares attributed to the thermonuclear runaway burning of carbon-rich material in the envelope of accreting neutron stars. By studying the details of the X-ray light curve, properties of carbon combustion can be determined. In particular, we show that the shape of the rise of the light curve is set by the slope of the temperature profile left behind by the carbon flame. We analyse Rossi X-ray Timing Explorer/Proportional Counter Array observations of 4U 1636-536 and separate the direct neutron star emission from evolving photoionized reflection and persistent spectral components. This procedure results in the highest quality light curve ever produced for the superburst rise and peak, and interesting behaviour is found in the tail. The rising light curve between 100 and 1000 s is inconsistent with the idea that the fuel burned locally and instantaneously everywhere, as assumed in some previous models. By fitting improved cooling models, we measure for the first time the radial temperature profile of the superbursting layer. We find d ln T/d ln P approximate to 1/4. Furthermore, 20 per cent of the fuel may be left unburned. This gives a new constraint on models of carbon burning and propagation in superbursts.
C1 [Keek, L.; Wolf, Z.; Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Cumming, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Suleimanov, V. F.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Suleimanov, V. F.] Kazan Volga Reg Fed Univ, Kazan 420008, Russia.
[Kuulkers, E.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain.
[Strohmayer, T. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Keek, L (reprint author), Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, 837 State St, Atlanta, GA 30332 USA.
EM l.keek@gatech.edu
FU NASA ADAP [NNX13AI47G]; NSF [AST 1008067]; National Sciences and
Engineering Research Council (NSERC) of Canada; German Research
Foundation (DFG) [WE 1312/48-1]; Australian Academy of Science;
Australian Research Council
FX We are grateful for discussions with E. F. Brown, A. Heger, and D. K.
Galloway. LK and DRB acknowledge support from NASA ADAP grant NNX13AI47G
and NSF award AST 1008067. AC was supported by the National Sciences and
Engineering Research Council (NSERC) of Canada. AC is an associate of
the CIFAR Cosmology and Gravity programme. VS was supported by German
Research Foundation (DFG) grant WE 1312/48-1. This paper uses
preliminary analysis results from the Multi-INstrument Burst ARchive
(MINBAR), which is supported under the Australian Academy of Science's
Scientific Visits to Europe program, and the Australian Research
Council's Discovery Projects and Future Fellowship funding schemes. We
made use of the EMCEE code by Foreman-Mackey et al., available at
http://dan.iel.fm/emcee.
NR 58
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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 DEC 21
PY 2015
VL 454
IS 4
BP 3559
EP 3566
DI 10.1093/mnras/stv2124
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600016
ER
PT J
AU Berney, S
Koss, M
Trakhtenbrot, B
Ricci, C
Lamperti, I
Schawinski, K
Balokovic, M
Crenshaw, DM
Fischer, T
Gehrels, N
Harrison, F
Hashimoto, Y
Ichikawa, K
Mushotzky, R
Oh, K
Stern, D
Treister, E
Ueda, Y
Veilleux, S
Winter, L
AF Berney, Simon
Koss, Michael
Trakhtenbrot, Benny
Ricci, Claudio
Lamperti, Isabella
Schawinski, Kevin
Balokovic, Mislav
Crenshaw, D. Michael
Fischer, Travis
Gehrels, Neil
Harrison, Fiona
Hashimoto, Yasuhiro
Ichikawa, Kohei
Mushotzky, Richard
Oh, Kyuseok
Stern, Daniel
Treister, Ezequiel
Ueda, Yoshihiro
Veilleux, Sylvain
Winter, Lisa
TI BAT AGN spectroscopic survey-II. X-ray emission and high-ionization
optical emission lines
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: nuclei; quasars: general
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE GROWTH; SEYFERT-GALAXIES; UNIFIED
SCHEMES; SKY SURVEY; LUMINOSITY; SPECTRA; REGION; CLASSIFICATION;
QUASARS
AB We investigate the relationship between X-ray and optical line emission in 340 nearby (z similar or equal to 0.04) AGN selected above 10 keV using Swift BAT. We find a weak correlation between the extinction corrected [O III] and hard X-ray luminosity (L-[O III](int) alpha L14-195) with a large scatter (R-Pear = 0.64, sigma = 0.62 dex) and a similarly large scatter with the intrinsic 2-10 keV to [O III] luminosities (R-Pear = 0.63, sigma = 0.63 dex). Correlations of the hard X-ray fluxes with the fluxes of high-ionization narrow lines ([O III], He II, [Ne III] and [Ne V]) are not significantly better than with the low-ionization lines (H alpha, [S II]). Factors like obscuration or physical slit size are not found to be a significant part of the large scatter. In contrast, the optical emission lines show much better correlations with each other (sigma = 0.3 dex) than with the X-ray flux. The inherent large scatter questions the common usage of narrow emission lines as AGN bolometric luminosity indicators and suggests that other issues such as geometrical differences in the scattering of the ionized gas or long-term AGN variability are important.
C1 [Berney, Simon; Koss, Michael; Trakhtenbrot, Benny; Lamperti, Isabella; Schawinski, Kevin; Oh, Kyuseok] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Ricci, Claudio] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Balokovic, Mislav; Harrison, Fiona] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Crenshaw, D. Michael; Fischer, Travis] Georgia State Univ, Dept Phys & Astron, Astron Off, Atlanta, GA 30303 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hashimoto, Yasuhiro] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 11677, Taiwan.
[Ichikawa, Kohei; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
[Mushotzky, Richard; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Treister, Ezequiel] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Winter, Lisa] Atmospher & Environm Res, Lexington, MA 02421 USA.
RP Berney, S (reprint author), ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
EM mike.koss@phys.ethz.ch
OI Schawinski, Kevin/0000-0001-5464-0888; Trakhtenbrot,
Benny/0000-0002-3683-7297
FU Swiss National Science Foundation (SNSF) [PZ00P2_154799/1]; SNSF [PP00P2
138979/1]; Center of Excellence in Astrophysics and Associated
Technologies [PFB 06]; FONDECYT [1120061]; CONICYT Anillo project
[ACT1101]; NASA; NASA Headquarters under the NASA Earth and Space
Science Fellowship Program [NNX14AQ07H]; CONICYT-Chile EMBIGGEN Anillo
[ACT1101]; Gemini programmes [GN-2009B-Q-114, GN-2010A-Q-35,
GN-2011A-Q-81, GN-2011B-Q-96, GN-2012A-Q-28, GN-2012B-Q-25,
GS-2010A-Q-54, GS-2011B-Q80]; Alfred P. Sloan Foundation; National
Science Foundation; US Department of Energy Office of Science; National
Aeronautics and Space Administration; US Department of Energy; 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
FX MK acknowledges support from the Swiss National Science Foundation
(SNSF) through the Ambizione fellowship grant PZ00P2_154799/1. MK and KS
acknowledge support from SNSF grant PP00P2 138979/1. Support for the
work of ET was provided by the Center of Excellence in Astrophysics and
Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061
and by the CONICYT Anillo project ACT1101. The work of DS was carried
out at Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA. MB acknowledges support from NASA
Headquarters under the NASA Earth and Space Science Fellowship Program,
grant NNX14AQ07H. CR acknowledges financial support from the
CONICYT-Chile EMBIGGEN Anillo (grant ACT1101). Based on observations
obtained at the Gemini Observatory, 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, Tecnologia e Innovacion Productiva (Argentina). Data in this
paper were acquired through the Gemini Science Archive and processed
using the Gemini IRAP package and Gemini PYTHON. Data from Gemini
programmes GN-2009B-Q-114, GN-2010A-Q-35, GN-2011A-Q-81, GN-2011B-Q-96,
GN-2012A-Q-28, GN-2012B-Q-25, GS-2010A-Q-54, and GS-2011B-Q80 were used
in this publication. We acknowledge the work that the Swift BAT team has
done to make this work possible. The Kitt Peak National Observatory
observations were obtained using MDTAC time as part of the thesis of MK
and LW at the University of Maryland. Kitt Peak National Observatory,
National Optical Astronomy Observatory, is operated by the Association
of Universities for Research in Astronomy (AURA), Inc., under
cooperative agreement with the National Science Foundation. 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. This research made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. Funding
for the SDSS and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, the US 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
website 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. 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 research made use of ASTROPY,
a community-developed core PYTHON package for Astronomy (Astropy
Collaboration 2013). 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 the SIMBAD data base, operated at CDS,
Strasbourg, France. This research made use of data and/or software
provided by 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 research made use of PySpeckit, an
open-source spectral analysis and plotting package for PYTHON hosted at
http://pyspeckit.bitbucket.org.
NR 57
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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 DEC 21
PY 2015
VL 454
IS 4
BP 3622
EP 3634
DI 10.1093/mnras/stv2181
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600022
ER
PT J
AU Fox, OD
Smith, N
Ammons, SM
Andrews, J
Bostroem, KA
Cenko, SB
Clayton, GC
Dwek, E
Filippenko, AV
Gallagher, JS
Kelly, PL
Mauerhan, JC
Miller, AA
Van Dyk, SD
AF Fox, Ori D.
Smith, Nathan
Ammons, S. Mark
Andrews, Jennifer
Bostroem, K. Azalee
Cenko, S. Bradley
Clayton, Geoffrey C.
Dwek, Eli
Filippenko, Alexei V.
Gallagher, Joseph S.
Kelly, Patrick L.
Mauerhan, Jon C.
Miller, Adam A.
Van Dyk, Schuyler D.
TI What powers the 3000-day light curve of SN 2006gy?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; supernovae: general; supernovae: individual: SN
2006gy; dust, extinction; infrared: stars
ID LUMINOUS SUPERNOVA; CIRCUMSTELLAR INTERACTION; IIN SUPERNOVAE; DUST
FORMATION; SPECTROSCOPY; STAR; PHOTOMETRY; EMISSION; 2005IP; 1987A
AB SN 2006gy was the most luminous supernova (SN) ever observed at the time of its discovery and the first of the newly defined class of superluminous supernovae (SLSNe). The extraordinary energetics of SN 2006gy and all SLSNe (>10(51) erg) require either atypically large explosion energies (e.g. pair-instability explosion) or the efficient conversion of kinetic into radiative energy (e.g. shock interaction). The mass-loss characteristics can therefore offer important clues regarding the progenitor system. For the case of SN 2006gy, both a scattered and thermal light echo from circumstellar material (CSM) have been reported at later epochs (day similar to 800), ruling out the likelihood of a pair-instability event and leading to constraints on the characteristics of the CSM. Owing to the proximity of the SN to the bright host-galaxy nucleus, continued monitoring of the light echo has not been trivial, requiring the high resolution offered by the Hubble Space Telescope (HST) or ground-based adaptive optics (AO). Here, we report detections of SN 2006gy using HST and Keck AO at similar to 3000 d post-explosion and consider the emission mechanism for the very late-time light curve. While the optical light curve and optical spectral energy distribution are consistent with a continued scattered-light echo, a thermal echo is insufficient to power the K'-band emission by day 3000. Instead, we present evidence for late-time infrared emission from dust that is radiatively heated by CSM interaction within an extremely dense dust shell, and we consider the implications on the CSM characteristics and progenitor system.
C1 [Fox, Ori D.; Filippenko, Alexei V.; Kelly, Patrick L.; Mauerhan, Jon C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fox, Ori D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Smith, Nathan; Andrews, Jennifer] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Ammons, S. Mark] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Bostroem, K. Azalee] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Cenko, S. Bradley; Dwek, Eli] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Clayton, Geoffrey C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Gallagher, Joseph S.] Univ Cincinnati, Blue Ash Coll, Blue Ash, OH 45236 USA.
[Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miller, Adam A.] CALTECH, Pasadena, CA 91125 USA.
[Van Dyk, Schuyler D.] CALTECH, IPAC, Pasadena, CA 91125 USA.
RP Fox, OD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM ofox@stsci.edu
OI Van Dyk, Schuyler/0000-0001-9038-9950
FU NASA [NAS5-26555]; W. M. Keck Foundation; NASA through STScI [GO-13287];
Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; US
Department of Energy through the Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]
FX This work is based on observations made with the NASA/ESA HST, obtained
from the Space Telescope Science Institute (STScI), which is operated by
the Association of Universities for Research in Astronomy (AURA), Inc.,
under NASA contract NAS5-26555. We are grateful to the STScI Help Desk
for their assistance with the HST data. 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 NASA; the observatory was made
possible by the generous financial support of the W. M. Keck Foundation.
The Keck observations were made possible by the ToO program. We thank
the staff of the Keck Observatory for their assistance with the
observations, as well as efforts by Sam Ragland and Mark Morris. Melissa
L. Graham and WeiKang Zheng helped obtain and reduce the Keck spectra.
We 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. We are most fortunate to have the
opportunity to conduct observations from this mountain.; Financial
support for ODF was provided by NASA through grant GO-13287 from STScI.
AVF and his group acknowledge generous financial assistance from the
Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant
AST-1211916. The research by SMA is supported by the US Department of
Energy through the Lawrence Livermore National Laboratory under Contract
DE-AC52-07NA27344.
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2015
VL 454
IS 4
BP 4366
EP 4378
DI 10.1093/mnras/stv2270
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600080
ER
PT J
AU Smith, LC
Lucas, PW
Pena, CC
Kurtev, R
Marocco, F
Jones, HRA
Beamin, JC
Napiwotzki, R
Borissova, J
Burningham, B
Faherty, J
Pinfield, DJ
Gromadzki, M
Ivanov, VD
Minniti, D
Stimson, W
Villanueva, V
AF Smith, L. C.
Lucas, P. W.
Pena, C. Contreras
Kurtev, R.
Marocco, F.
Jones, H. R. A.
Beamin, J. C.
Napiwotzki, R.
Borissova, J.
Burningham, B.
Faherty, J.
Pinfield, D. J.
Gromadzki, M.
Ivanov, V. D.
Minniti, D.
Stimson, W.
Villanueva, V.
TI Discovery of a brown dwarf companion to the A3V star beta Circini
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; brown dwarfs; stars: individual: beta Circini
ID PRE-MAIN-SEQUENCE; LOW-MASS STARS; STELLAR KINEMATIC GROUPS;
PLANET-FINDING CAMPAIGN; NEAR-INFRARED SPECTRA; A-TYPE STARS; ULTRACOOL
DWARFS; L/T TRANSITION; VAST SURVEY; VVV SURVEY
AB We report the discovery of an L dwarf companion to the A3V star beta Circini. VVV J151721.49-585131.5, or beta Cir B, was identified in a proper motion and parallax catalogue of the VISTA Variables in the Via Lactea survey as having near-infrared luminosity and colour indicative of an early L dwarf, and a proper motion and parallax consistent with that of beta Cir. The projected separation of similar to 3.6 arcmin corresponds to 6656 au, which is unusually wide. The most recent published estimate of the age of the primary combined with our own estimate based on newer isochrones yields an age of 370-500 Myr. The system therefore serves as a useful benchmark at an age greater than that of the Pleiades brown dwarfs and most other young L dwarf benchmarks. We have obtained a medium resolution echelle spectrum of the companion which indicates a spectral type of L1.0 +/- 0.5 and lacks the typical signatures of low-surface gravity seen in younger brown dwarfs. This suggests that signs of low-surface gravity disappear from the spectra of early L dwarfs by an age of similar to 370-500 Myr, as expected from theoretical isochrones. The mass of beta Cir B is estimated from the BHAC15 isochrones as 0.056 +/- 0.007 M-circle dot.
C1 [Smith, L. C.; Lucas, P. W.; Pena, C. Contreras; Marocco, F.; Jones, H. R. A.; Napiwotzki, R.; Burningham, B.; Pinfield, D. J.; Stimson, W.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Pena, C. Contreras; Minniti, D.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Pena, C. Contreras; Kurtev, R.; Beamin, J. C.; Borissova, J.; Gromadzki, M.; Villanueva, V.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Kurtev, R.; Borissova, J.; Gromadzki, M.; Villanueva, V.] Univ Valparaiso, inst Fis & Astron, Valparaiso, Chile.
[Beamin, J. C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Beamin, J. C.; Ivanov, V. D.] European So Observ, Santiago 19001, Chile.
[Burningham, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Faherty, J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Faherty, J.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10034 USA.
[Ivanov, V. D.] European So Observ, D-85748 Garching, Germany.
[Minniti, D.] Vatican Observ, I-V00120 Vatican City, Vatican.
RP Smith, LC (reprint author), Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
EM l.smith10@herts.ac.uk
OI Burningham, Ben/0000-0003-4600-5627
FU ESO Public Survey programme [179.B-2002]; FONDAP Center for Astrophysics
[15010003]; BASAL CATA Center for Astrophysics and Associated
Technologies [PFB-06]; FONDECYT from CONICYT; Science & Technology
Facilities Research Council (STFC) of the UK; consolidated grant
[ST/J001333/1]; STFC; Ministry of Economy, Development, and Tourism's
Millennium Science Initiative [IC120009]; CONICYT REDES [140042];
Fondecyt [1130140, 1130196, 1120601]; Committee ESO; Government of Chile
FX We would like to thank the anonymous referee for a swift and useful
report. We are grateful to K. Allers for supplying the low gravity BD
spectra. LS is grateful to N. Deacon and M. Irwin for helpful viva
comments, and R. Smart for various useful discussions. We acknowledge
use of data from the ESO Public Survey programme ID 179.B-2002 taken
with the VISTA telescope, data products from CASU, and funding from the
FONDAP Center for Astrophysics 15010003, the BASAL CATA Center for
Astrophysics and Associated Technologies PFB-06, the FONDECYT from
CONICYT. This research uses data gathered with the 6.5 metre Magellan
Telescopes located at Las Campanas Observatory, Chile. LS acknowledges a
studentship funded by the Science & Technology Facilities Research
Council (STFC) of the UK; PWL acknowledge the support of a consolidated
grant (ST/J001333/1) also funded by STFC. Support for RK, DM, MG, VV,
CCP, JB and JCB is provided by the Ministry of Economy, Development, and
Tourism's Millennium Science Initiative through grant IC120009, awarded
to The Millennium Institute of Astrophysics (MAS), they also acknowledge
CONICYT REDES No. 140042 project. RK and DM are supported by Fondecyt
Reg. No. 1130140 and No. 1130196, respectively. MG acknowledges support
from Joined Committee ESO and Government of Chile 2014 and Fondecyt
Regular No. 1120601. This research has made use of the SIMBAD data base
and VizieR catalogue access tool, operated at CDS, Strasbourg, France;
NASA's Astrophysics Data System Bibliographic Services and the SpeX
Prism Spectral Libraries, maintained by Adam Burgasser at
pono.ucsd.edu/similar to adam/browndwarfs/spexprism.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2015
VL 454
IS 4
BP 4476
EP 4483
DI 10.1093/mnras/stv2290
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7RK
UT WOS:000368001600088
ER
PT J
AU Abeysekara, AU
Archambault, S
Archer, A
Aune, T
Barnacka, A
Benbow, W
Bird, R
Biteau, J
Buckley, JH
Bugaev, V
Cardenzana, JV
Cerruti, M
Chen, X
Christiansen, JL
Ciupik, L
Connolly, MP
Coppi, P
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Errando, M
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
Khassen, Y
Kieda, D
Krause, M
Krennrich, F
Kumar, S
Lang, MJ
Maier, G
McArthur, S
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
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
Rousselle, J
Santander, M
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Todd, NW
Tucci, JV
Tyler, J
Vassiliev, VV
Vincent, S
Wakely, SP
Weiner, OM
Weinstein, A
Wilhelm, A
Williams, DA
Zitzer, B
Smith, PS
Holoien, TWS
Prieto, JL
Kochanek, CS
Stanek, KZ
Shappee, B
Hovatta, T
Max-Moerbeck, W
Pearson, TJ
Reeves, RA
Richards, JL
Readhead, ACS
Madejski, GM
Djorgovski, SG
Drake, AJ
Graham, MJ
Mahabal, A
AF Abeysekara, A. U.
Archambault, S.
Archer, A.
Aune, T.
Barnacka, A.
Benbow, W.
Bird, R.
Biteau, J.
Buckley, J. H.
Bugaev, V.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Christiansen, J. L.
Ciupik, L.
Connolly, M. P.
Coppi, P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Errando, M.
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.
Khassen, Y.
Kieda, D.
Krause, M.
Krennrich, F.
Kumar, S.
Lang, M. J.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
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.
Rousselle, J.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Todd, N. W.
Tucci, J. V.
Tyler, J.
Vassiliev, V. V.
Vincent, S.
Wakely, S. P.
Weiner, O. M.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
Smith, P. S.
Holoien, T. W. -S.
Prieto, J. L.
Kochanek, C. S.
Stanek, K. Z.
Shappee, B.
Hovatta, T.
Max-Moerbeck, W.
Pearson, T. J.
Reeves, R. A.
Richards, J. L.
Readhead, A. C. S.
Madejski, G. M.
Djorgovski, S. G.
Drake, A. J.
Graham, M. J.
Mahabal, A.
CA VERITAS
SPOL
ASAS-SN
OVRO
NuSTAR
CRTS
TI GAMMA-RAYS FROM THE QUASAR PKS 1441+25: STORY OF AN ESCAPE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; diffuse radiation; gamma rays: galaxies;
quasars: individual (PKS 1441+25-VER J1443+250); radiation mechanisms:
non-thermal
ID EXTRAGALACTIC BACKGROUND LIGHT; COMPLETE SAMPLE; FERMI BLAZARS; SPECTRA;
VARIABILITY; TELESCOPE; RADIATION; EMISSION; MISSION; ABSORPTION
AB Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma-rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EBL), or the radiation near the supermassive black hole lying at the jet's base. VERITAS detected gamma-ray emission up to similar to 200 GeV from PKS 1441+25 (z = 0.939) during 2015 April, a period of high activity across all wavelengths. This observation of PKS 1441+25 suggests that the emission region is located thousands of Schwarzschild radii away from the black hole. The gamma-ray detection also sets a stringent upper limit on the near-ultraviolet to near-infrared EBL intensity, suggesting that galaxy surveys have resolved most, if not all, of the sources of the EBL at these wavelengths.
C1 [Abeysekara, A. U.; Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Archer, A.; Buckley, J. H.; Bugaev, V.; Errando, M.; Todd, N. W.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Aune, T.; Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Cardenzana, J. V.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; De Bhroithe, A. O'Faolain; Pohl, M.; Telezhinsky, I.; Vincent, S.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Christiansen, J. L.] DESY, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Coppi, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.; Richards, J. L.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Dickinson, H. J.; Dumm, J.; Fleischhack, H.; Fortson, L.; Shahinyan, K.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Errando, M.; Mukherjee, R.; Santander, M.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Holder, J.; Kumar, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Humensky, T. B.; Nieto, D.; Petrashyk, A.; Weiner, O. M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Kaaret, P.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Park, N.; Wakely, S. P.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Perkins, J. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Reynolds, P. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, A. W.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Zitzer, B.] Univ Maryland, College Pk, MD 20742 USA.
[Smith, P. S.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Holoien, T. W. -S.; Kochanek, C. S.; Stanek, K. Z.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Holoien, T. W. -S.; Kochanek, C. S.; Stanek, K. Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Prieto, J. L.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Prieto, J. L.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
[Shappee, B.] Millennium Inst Astrophys, Santiago, Chile.
[Hovatta, T.] Carnegie Observ, Pasadena, CA 91101 USA.
[Max-Moerbeck, W.] Aalto Univ, Metsahovi Radio Observ, FI-02540 Kylmala, Finland.
[Pearson, T. J.; Readhead, A. C. S.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Reeves, R. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Madejski, G. M.] Univ Concepcion, Dept Astron, CePIA, Concepcion, Chile.
[Madejski, G. M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Djorgovski, S. G.; Drake, A. J.; Graham, M. J.; Mahabal, A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
CALTECH, Pasadena, CA 91125 USA.
RP Abeysekara, AU (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
EM jbiteau@ucsc.edu; matteo.cerruti@cfa.harvard.edu;
errando@astro.columbia.edu; caajohns@ucsc.edu; mark.lang@nuigalway.ie
RI Nieto, Daniel/J-7250-2015; Pearson, Timothy/N-2376-2015;
OI Nieto, Daniel/0000-0003-3343-0755; Pearson, Timothy/0000-0001-5213-6231;
Pueschel, Elisa/0000-0002-0529-1973; Errando, Manel/0000-0002-1853-863X;
Lang, Mark/0000-0003-4641-4201; 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; NASA Swift GI
grant [NNX15AR38G]; LCOGT; NSF [AST-1313422, AST-1413600, AST-0808050,
AST-1109911]; Mt. Cuba Astronomical Foundation; OSU/CCAPP; MAS/Chile;
NASA Fermi GI grant [NNX12AO93G]; NASA [NNX08AW31G, NNX11A043G]
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, with additional support
from NASA Swift GI grant NNX15AR38G. 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.; ASAS-SN thanks
LCOGT, NSF, Mt. Cuba Astronomical Foundation, OSU/CCAPP and MAS/Chile
for their support.; The observations at Steward Observatory are funded
through NASA Fermi GI grant NNX12AO93G.; CRTS is supported by the NSF
grants AST-1313422 and AST-1413600.; The OVRO 40-m monitoring program is
supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF
grants AST-0808050 and AST-1109911.
NR 42
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2015
VL 815
IS 2
AR L22
DI 10.1088/2041-8205/815/2/L22
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC2XI
UT WOS:000369081700006
ER
PT J
AU Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Banerjee, B
Bangale, P
De Almeida, UB
Barrio, JA
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, F
Prester, DD
Dorner, D
Doro, M
Einecke, S
Glawion, DE
Elsaesser, D
Fernandez-Barral, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Giammaria, P
Godinovic, 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
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, M
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palacio, J
Palatiello, M
Paneque, D
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
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
Ajello, M
Baldini, L
Barbiellini, G
Bastieri, D
Gonzalez, JB
Bellazzini, R
Bissaldi, E
Blandford, RD
Bonino, R
Bregeon, J
Bruel, P
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Chiang, J
Chiaro, G
Ciprini, S
D'Ammando, F
de Palma, F
Desiante, R
Di Venere, L
Dominguez, A
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Grenier, IA
Guiriec, S
Hays, E
Hewitt, JW
Jogler, T
Kuss, M
Larsson, S
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Maldera, S
Mayer, M
Mazziotta, MN
McEnery, JE
Mirabal, N
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Nuss, E
Ojha, R
Ohsugi, T
Omodei, N
Orlando, E
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Tajima, H
Takahashi, H
Thayer, JB
Thompson, DJ
Troja, E
Wood, KS
Balokovic, M
Berdyugin, A
Carraminana, A
Carrasco, L
Chavushyan, V
Ramazani, VF
Feige, M
Haarto, S
Haeusner, P
Hovatta, T
Kania, J
Klamt, J
Lahteenmaki, A
Leon-Tavares, J
Lorey, C
Pacciani, L
Porras, A
Recillas, E
Reinthal, R
Tornikoski, M
Wolfert, D
Zottmann, N
AF Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Banerjee, B.
Bangale, P.
De Almeida, U. Barres
Barrio, J. A.
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, F.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Garcia Lopez, R. J.
Garczarczyk, M.
Garrido Terrats, D.
Gaug, M.
Giammaria, P.
Godinovic, 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.
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.
Nievas Rosillo, M.
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palacio, J.
Palatiello, M.
Paneque, D.
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.
Garcia, J. Rodriguez
Saito, T.
Satalecka, K.
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.
Ajello, M.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Becerra Gonzalez, J.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bonino, R.
Bregeon, J.
Bruel, P.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Chiang, J.
Chiaro, G.
Ciprini, S.
D'Ammando, F.
de Palma, F.
Desiante, R.
Di Venere, L.
Dominguez, A.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Grenier, I. A.
Guiriec, S.
Hays, E.
Hewitt, J. W.
Jogler, T.
Kuss, M.
Larsson, S.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Maldera, S.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Mirabal, N.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Nuss, E.
Ojha, R.
Ohsugi, T.
Omodei, N.
Orlando, E.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Tajima, H.
Takahashi, H.
Thayer, J. B.
Thompson, D. J.
Troja, E.
Wood, K. S.
Balokovic, M.
Berdyugin, A.
Carraminana, A.
Carrasco, L.
Chavushyan, V.
Ramazani, V. Fallah
Feige, M.
Haarto, S.
Haeusner, P.
Hovatta, T.
Kania, J.
Klamt, J.
Lahteenmaki, A.
Leon-Tavares, J.
Lorey, C.
Pacciani, L.
Porras, A.
Recillas, E.
Reinthal, R.
Tornikoski, M.
Wolfert, D.
Zottmann, N.
CA MAGIC Collaboration
Fermi-LAT Collaboration
TI VERY HIGH ENERGY gamma-RAYS FROM THE UNIVERSE'S MIDDLE AGE: DETECTION OF
THE z=0.940 BLAZAR PKS 1441+25 WITH MAGIC
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; galaxies: active; galaxies: jets; gamma
rays: galaxies; quasars: individual (PKS 1441+25)
ID EXTRAGALACTIC BACKGROUND LIGHT; LARGE-AREA TELESCOPE;
COMPTON-SCATTERING; RADIATION-FIELDS; SOURCE CATALOG; LINE BLAZARS;
SPECTRA; ABSORPTION; EMISSION; MISSION
AB The flat-spectrum radio quasar PKS 1441+25 at a redshift of z = 0.940 is detected between 40 and 250 GeV with a significance of 25.5 sigma using the MAGIC telescopes. Together with the gravitationally lensed blazar QSO. B0218 +357 (z = 0.944), PKS. 1441+25 is the most distant very high energy (VHE) blazar detected to date. The observations were triggered by an outburst in 2015 April seen at GeV energies with the Large Area Telescope on board Fermi. Multi-wavelength observations suggest a subdivision of the high state into two distinct flux states. In the band covered by MAGIC, the variability timescale is estimated to be 6.4 +/- 1.9 days. Modeling the broadband spectral energy distribution with an external Compton model, the location of the emitting region is understood as originating in the jet outside the broad-line region (BLR) during the period of high activity, while being partially within the BLR during the period of low (typical) activity. The observed VHE spectrum during the highest activity is used to probe the extragalactic background light at an unprecedented distance scale for ground-based gamma-ray astronomy.
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[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, F.; 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.
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[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
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[Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Elsaesser, D.; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambient & Tecnol, E-28040 Madrid, Spain.
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[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.
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[Moroni, P. G. Prada; Shore, S. N.; Baldini, L.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy.
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[de Palma, F.] Univ Telemat Pegaso, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
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RP Ahnen, ML (reprint author), ETH, CH-8093 Zurich, Switzerland.
EM manganaro@iac.es; miguelnievas@ucm.es; fabrizio.tavecchio@brera.inaf.it;
josefa.becerra@nasa.gov
RI Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Orlando,
E/R-5594-2016; Bonino, Raffaella/S-2367-2016; Miranda, Jose
Miguel/F-2913-2013; Delgado, Carlos/K-7587-2014; Barrio,
Juan/L-3227-2014; GAug, Markus/L-2340-2014; Martinez Rodriguez,
Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Di Venere,
Leonardo/C-7619-2017; Lahteenmaki, Anne/L-5987-2013; Temnikov,
Petar/L-6999-2016; Reimer, Olaf/A-3117-2013; giglietto,
nicola/I-8951-2012; Font, Lluis/L-4197-2014; Moskalenko,
Igor/A-1301-2007; Poutanen, Juri/H-6651-2016; Nievas Rosillo,
Mireia/K-9738-2014; Manganaro, Marina/B-7657-2011; Lopez Moya,
Marcos/L-2304-2014; Bissaldi, Elisabetta/K-7911-2016; Maneva,
Galina/L-7120-2016; Fonseca Gonzalez, Maria Victoria/I-2004-2015;
OI Torres, Diego/0000-0002-1522-9065; Miranda, Jose
Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Barrio,
Juan/0000-0002-0965-0259; GAug, Markus/0000-0001-8442-7877; Cortina,
Juan/0000-0003-4576-0452; Di Venere, Leonardo/0000-0003-0703-824X;
Temnikov, Petar/0000-0002-9559-3384; Reimer, Olaf/0000-0001-6953-1385;
giglietto, nicola/0000-0002-9021-2888; Font, Lluis/0000-0003-2109-5961;
Moskalenko, Igor/0000-0001-6141-458X; Poutanen,
Juri/0000-0002-0983-0049; Nievas Rosillo, Mireia/0000-0002-8321-9168;
Manganaro, Marina/0000-0003-1530-3031; Lopez Moya,
Marcos/0000-0002-8791-7908; Bissaldi, Elisabetta/0000-0001-9935-8106;
Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Sgro',
Carmelo/0000-0001-5676-6214
FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund
SNF; ERDF under the Spanish MINECO [FPA2012-39502]; ERDF under the
Spanish MECD [FPU13/00618]; Japanese JSPS; Japanese MEXT; Centro de
Excelencia Severo Ochoa project of the Spanish Consolider-Ingenio
programme [SEV-2012-0234]; CPAN project of the Spanish
Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the
Spanish Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland
[268740]; Croatian Science Foundation (HrZZ) [09/176]; University of
Rijeka [13.12.1.3.02]; DFG Collaborative Research Centers [SFB823/C4,
SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; NASA (United
States); DOE (United States); CEA/Irfu (France); IN2P3/CNRS (France);
ASI (Italy); INFN (Italy); MEXT (Japan); KEK (Japan); JAXA (Japan); K.A.
Wallenberg Foundation; Swedish Research Council; National Space Board
(Sweden); INAF (Italy); CNES (France); PRIN-INAF
FX We would like to thank the Instituto 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 (FPA2012-39502) and MECD (FPU13/00618), 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 SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant
745/N-HESS-MAGIC/2010/0.; The Fermi-LAT Collaboration acknowledges
support for LAT development, operation and data analysis from NASA and
DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN
(Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg
Foundation, the Swedish Research Council and the National Space Board
(Sweden). Science analysis support in the operations phase from INAF
(Italy) and CNES (France) is also gratefully acknowledged.; We thank the
Swift team duty scientists and science planners. L.P. acknowledges the
PRIN-INAF 2014 financial support.
NR 40
TC 10
Z9 10
U1 4
U2 17
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 DEC 20
PY 2015
VL 815
IS 2
AR L23
DI 10.1088/2041-8205/815/2/L23
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC2XI
UT WOS:000369081700007
ER
PT J
AU Khan, R
Adams, SM
Stanek, KZ
Kochanek, CS
Sonneborn, G
AF Khan, Rubab
Adams, Scott M.
Stanek, K. Z.
Kochanek, C. S.
Sonneborn, G.
TI DISCOVERY OF FIVE CANDIDATE ANALOGS FOR eta CARINAE IN NEARBY GALAXIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: evolution; stars: individual (eta Carinae); stars: massive;
stars: mass-loss
ID MASSIVE STARS; IMAGE SUBTRACTION; SPACE-TELESCOPE; GREAT ERUPTION;
CORE-COLLAPSE; LIGHT ECHOES; POINT-SOURCE; CAR ANALOGS; SN 2009IP;
SUPERNOVA
AB The late-stage evolution of very massive stars such as eta Carinae may be dominated by episodic mass ejections that may later lead to Type II superluminous supernova (SLSN-II; e.g., SN 2006gy). However, as long as eta Car is one of a kind, it is nearly impossible to quantitatively evaluate these possibilities. Here, we announce the discovery of five objects in the nearby (similar to 4-8 Mpc) massive star-forming galaxies M51, M83, M101, and NGC 6946 that have optical through mid-infrared (mid-IR) photometric properties consistent with the hitherto unique eta Car. The Spitzer mid-IR spectral energy distributions of these L-bol similar or equal to 3-8 x 10(6) L-circle dot objects rise steeply in the 3.6-8 mu m bands and then turn over between 8 and 24 mu m, indicating the presence of warm (similar to 400-600 K) circumstellar dust. Their optical counterparts in HST images are similar to 1.5-2 dex fainter than their mid-IR peaks and require the presence of similar to 5-10M(circle dot) of obscuring material. Our finding implies that the rate of eta Car-like events is a fraction f = 0.094 (0.040 < f < 0.21 at 90% confidence) of the core-collapse supernova (ccSN) rate. If there is only one eruption mechanism and Type II superluminous supernovae are due to ccSNe occurring inside these dense shells, then the ejection mechanism is likely associated with the onset of carbon burning (similar to 10(3)-10(4) years), which is also consistent with the apparent ages of massive Galactic shells.
C1 [Khan, Rubab] NASA, Goddard Space Flight Ctr, MC 665,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Khan, Rubab; Sonneborn, G.] ORAU, NASA Postdoctoral Program, Oak Ridge, TN 37831 USA.
[Adams, Scott M.; Stanek, K. Z.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Stanek, K. Z.; Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
RP Khan, R (reprint author), NASA, Goddard Space Flight Ctr, MC 665,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM rubab.m.khan@nasa.gov; sadams@astronomy.ohio-state.edu;
kstanek@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu;
george.sonneborn-1@nasa.gov
FU NASA Postdoctoral Program; Presidential Fellowship at The Ohio State
University; NSF [AST-151592, AST-1515876]
FX We thank the referee for helpful comments. R.K. is supported by a JWST
Fellowship awarded through the NASA Postdoctoral Program. S.M.A. is
supported by a Presidential Fellowship at The Ohio State University.
K.Z.S. is supported in part by NSF grant AST-151592. C.S.K. is supported
by NSF grant AST-1515876. This research has made use of observations
made with the Spitzer Space Telescope, which is operated by the JPL and
Caltech under a contract with NASA; observations made with the NASA/ESA
Hubble Space Telescope and obtained from the Hubble Legacy Archive,
which is a collaboration between the STScI/NASA, ST-ECF/ESA, and the
CADC/NRC/CSA; and the VizieR catalog access tool, CDS, Strasbourg,
France.
NR 43
TC 3
Z9 3
U1 1
U2 5
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 DEC 20
PY 2015
VL 815
IS 2
AR L18
DI 10.1088/2041-8205/815/2/L18
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC2XI
UT WOS:000369081700002
ER
PT J
AU Bussmann, RS
Riechers, D
Fialkov, A
Scudder, J
Hayward, CC
Cowley, WI
Bock, J
Calanog, J
Chapman, SC
Cooray, A
De Bernardis, F
Farrah, D
Fu, H
Gavazzi, R
Hopwood, R
Ivison, RJ
Jarvis, M
Lacey, C
Loeb, A
Oliver, SJ
Perez-Fournon, I
Rigopoulou, D
Roseboom, IG
Scott, D
Smith, AJ
Vieira, JD
Wang, L
Wardlow, J
AF Bussmann, R. S.
Riechers, D.
Fialkov, A.
Scudder, J.
Hayward, C. C.
Cowley, W. I.
Bock, J.
Calanog, J.
Chapman, S. C.
Cooray, A.
De Bernardis, F.
Farrah, D.
Fu, Hai
Gavazzi, R.
Hopwood, R.
Ivison, R. J.
Jarvis, M.
Lacey, C.
Loeb, A.
Oliver, S. J.
Perez-Fournon, I.
Rigopoulou, D.
Roseboom, I. G.
Scott, Douglas
Smith, A. J.
Vieira, J. D.
Wang, L.
Wardlow, J.
TI HERMES: ALMA IMAGING OF HERSCHEL-SELECTED DUSTY STAR-FORMING GALAXIES
(vol 812, pg 43, 2015)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Bussmann, R. S.; Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Fialkov, A.] Ecole Normale Super, CNRS, Dept Phys, F-75005 Paris, France.
[Scudder, J.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Hayward, C. C.] CALTECH, TAPIR 350 17, Pasadena, CA 91125 USA.
[Hayward, C. C.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cowley, W. I.; Lacey, C.; Wang, L.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
[Bock, J.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Calanog, J.; Cooray, A.; De Bernardis, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Gavazzi, R.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarvis, M.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Jarvis, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
[Perez-Fournon, I.] IAC, E-38200 Tenerife, Spain.
[Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Wang, L.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Wardlow, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
RP Bussmann, RS (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA.
RI Ivison, R./G-4450-2011; Wardlow, Julie/C-9903-2015
OI Ivison, R./0000-0001-5118-1313; Wardlow, Julie/0000-0003-2376-8971
NR 1
TC 0
Z9 0
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 DEC 20
PY 2015
VL 815
IS 2
AR 135
DI 10.1088/0004-637X/815/2/135
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300055
ER
PT J
AU Hakkila, J
Lien, A
Sakamoto, T
Morris, D
Neff, JE
Giblin, TW
AF Hakkila, Jon
Lien, Amy
Sakamoto, Takanori
Morris, David
Neff, James E.
Giblin, Timothy W.
TI SWIFT OBSERVATIONS OF GAMMA-RAY BURST PULSE SHAPES: GRB PULSE SPECTRAL
EVOLUTION CLARIFIED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; methods: statistical
ID HARDNESS EVOLUTION; PROMPT EMISSION; INTERNAL SHOCK; FLARES; LONG;
COMPONENT; BRIGHT; SHELLS; WIDTH; LAG
AB Isolated Swift gamma-ray burst (GRB) pulses, like their higher-energy BATSE counterparts, emit the bulk of their pulsed emission as a hard-to-soft component that can be fitted by the Norris et al. empirical pulse model. This signal is overlaid by a fainter, three-peaked signal that can be modeled by the residual fit of Hakkila & Preece: the two fits combine to reproduce GRB pulses with distinctive three-peaked shapes. The precursor peak appears on or before the pulse rise and is often the hardest component, the central peak is the brightest, and the decay peak converts exponentially decaying emission into a long, soft, power-law tail. Accounting for systematic instrumental differences, the general characteristics of the fitted pulses are remarkably similar. Isolated GRB pulses are dominated by hard-to-soft evolution; this is more pronounced for asymmetric pulses than for symmetric ones. Isolated GRB pulses can also exhibit intensity tracking behaviors that, when observed, are tied to the timing of the three peaks: pulses with the largest maximum hardnesses are hardest during the precursor, those with smaller maximum hardnesses are hardest during the central peak, and all pulses can re-harden during the central peak and/or during the decay peak. Since these behaviors are essentially seen in all isolated pulses, the distinction between "hard-to-soft and "intensity-tracking" pulses really no longer applies. Additionally, the triple-peaked nature of isolated GRB pulses seems to indicate that energy is injected on three separate occasions during the pulse duration: theoretical pulse models need to account for this.
C1 [Hakkila, Jon] Univ Charleston South Carolina, Coll Charleston, Charleston, SC 29424 USA.
[Lien, Amy; Sakamoto, Takanori] CRESST, Greenbelt, MD 20771 USA.
[Lien, Amy; Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lien, Amy] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Sakamoto, Takanori] Aoyama Gakuin Univ, Dept Math & Phys, Tokyo 150, Japan.
[Morris, David] Univ Virgin Isl, Dept Phys, St Thomas, VI 00802 USA.
[Neff, James E.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Giblin, Timothy W.] US Air Force Acad, Dept Phys, Colorado Springs, CO 80840 USA.
RP Hakkila, J (reprint author), Univ Charleston South Carolina, Coll Charleston, Charleston, SC 29424 USA.
EM hakkilaj@cofc.edu
FU NASA EPSCoR grant [NNX13AD28A]
FX We would like to acknowledge the helpful comments of the anonymous
referee, as these greatly helped to improve the manuscript. This work
has been supported by NASA EPSCoR grant NNX13AD28A.
NR 30
TC 1
Z9 1
U1 0
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 DEC 20
PY 2015
VL 815
IS 2
AR 134
DI 10.1088/0004-637X/815/2/134
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300054
ER
PT J
AU Hasegawa, Y
Takeuchi, T
AF Hasegawa, Yasuhiro
Takeuchi, Taku
TI VISCOUS INSTABILITY TRIGGERED BY LAYERED ACCRETION IN PROTOPLANETARY
DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD);
protoplanetary disks; turbulence
ID WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY; T TAURI DISKS;
MAGNETOROTATIONAL INSTABILITY; NONLINEAR EVOLUTION; DEAD ZONES;
AMBIPOLAR DIFFUSION; PROTOSTELLAR DISKS; DRIVEN ACCRETION; IONIZATION
STATE
AB Layered accretion is one of the inevitable ingredients in protoplanetary disks when disk turbulence is excited by magnetorotational instabilities (MRIs). In the accretion, disk surfaces where MRIs fully operate have a high value of disk accretion rate ((M) over dot), while the disk midplane where MRIs are generally quenched ends up with a low value of (M) over dot . Significant progress on understanding MRIs has recently been made by a number of dedicated MHD simulations, which requires improvement of the classical treatment of a in 1D disk models. To this end, we obtain a new expression of alpha by utilizing an empirical formula that is derived from recent MHD simulations of stratified disks with ohmic diffusion. It is interesting that this new formulation can be regarded as a general extension of the classical alpha. Armed with the new a, we perform a linear stability analysis of protoplanetary disks that undergo layered accretion, and we find that a viscous instability can occur around the outer edge of dead zones. Disks become stable in using the classical a. We identify that the difference arises from Sigma-dependence of (M) over dot; whereas Sigma is uniquely determined for a given value of M in the classical approach, the new approach leads to (M) over dot that is a multivalued function of Sigma. We confirm our finding both by exploring a parameter space and by performing the 1D, viscous evolution of disks. We finally discuss other nonideal MHD effects that are not included in our analysis but may affect our results.
C1 [Hasegawa, Yasuhiro] Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan.
[Hasegawa, Yasuhiro] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takeuchi, Taku] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
RP Hasegawa, Y (reprint author), Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan.
EM yasuhiro@caltech.edu
FU MEXT of Japan [23103005, 26103704, 26400224]; Jet Propulsion Laboratory,
California Institute of Technology; East Asia Core Observatories
Association
FX The authors thank Mario Flock, Satoshi Okuzumi, and Neal Turner for
stimulating discussions, and an anonymous referee for useful comments on
our manuscript. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Y.H. is
currently supported by the Jet Propulsion Laboratory, California
Institute of Technology, and has previously been by an EACOA Fellowship
that is supported by East Asia Core Observatories Association, which
consists of the Academia Sinica Institute of Astronomy and Astrophysics,
the National Astronomical Observatory of Japan, the National
Astronomical Observatory of China, and the Korea Astronomy and Space
Science Institute. T.T. is supported by Grants-in-Aid for Scientific
Research, Nos. 23103005, 26103704, and 26400224, from MEXT of Japan.
NR 63
TC 1
Z9 1
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 DEC 20
PY 2015
VL 815
IS 2
AR 99
DI 10.1088/0004-637X/815/2/99
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300019
ER
PT J
AU Morley, CV
Fortney, JJ
Marley, MS
Zahnle, K
Line, M
Kempton, E
Lewis, N
Cahoy, K
AF Morley, Caroline V.
Fortney, Jonathan J.
Marley, Mark S.
Zahnle, Kevin
Line, Michael
Kempton, Eliza
Lewis, Nikole
Cahoy, Kerri
TI THERMAL EMISSION AND REFLECTED LIGHT SPECTRA OF SUPER EARTHS WITH FLAT
TRANSMISSION SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(GJ 1214b)
ID EXTRASOLAR GIANT PLANETS; EXOPLANET GJ 1214B; SYSTEMATIC RETRIEVAL
ANALYSIS; COLLISION-INDUCED ABSORPTION; HUBBLE-SPACE-TELESCOPE; BROWN
DWARFS; LINE LISTS; 1500 K; ATMOSPHERIC CHEMISTRY; MULTIPLE-SCATTERING
AB Planets larger than Earth and smaller than Neptune are some of the most numerous in the galaxy, but observational efforts to understand this population have proved challenging because optically thick clouds or hazes at high altitudes obscure molecular features. We present models of super Earths that include thick clouds and hazes and predict their transmission, thermal emission, and reflected light spectra. Very thick, lofted clouds of salts or sulfides in high metallicity (1000x solar) atmospheres create featureless transmission spectra in the near-infrared. Photochemical hazes with a range of particle sizes also create featureless transmission spectra at lower metallicities. Cloudy thermal emission spectra have muted features more like blackbodies, and hazy thermal emission spectra have emission features caused by an inversion layer at altitudes where the haze forms. Close analysis of reflected light from warm (similar to 400-800 K) planets can distinguish cloudy spectra, which have moderate albedos (0.05-0.20), from hazy models, which are very dark (0.0-0.03). Reflected light spectra of cold planets (similar to 200 K) accessible to a space-based visible light coronagraph will have high albedos and large molecular features that will allow them to be more easily characterized than the warmer transiting planets. We suggest a number of complementary observations to characterize this population of planets, including transmission spectra of hot (greater than or similar to 1000 K) targets, thermal emission spectra of warm targets using the James Webb Space Telescope, high spectral resolution (R similar to 10(5)) observations of cloudy targets, and reflected light spectral observations of directly imaged cold targets. Despite the dearth of features observed in super Earth transmission spectra to date, different observations will provide rich diagnostics of their atmospheres.
C1 [Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, Mark S.; Zahnle, Kevin; Line, Michael] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Kempton, Eliza] Grinnell Coll, Grinnell, IA 50112 USA.
[Lewis, Nikole] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Cahoy, Kerri] MIT, Cambridge, MA 02139 USA.
RP Morley, CV (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM cmorley@ucolick.org
OI Marley, Mark/0000-0002-5251-2943
FU HST Theory Grant [HST-AR-13918.002-A]; Hubble grants [HST-GO-13501.06-A,
HST-GO-13665.004-A]; NSF [AST-1312545]; NASA Origins program; NASA
through Hubble Fellowship grant - Space Telescope Science Institute
[51362]; NASA [NAS 5-26555]
FX We thank the anonymous referee for their exceptionally helpful report
which improved the manuscript. We also acknowledge the work to reformat
our opacity database for the new radiative transfer code by high school
students Anjini Karthik and Matthew Huang during Summer 2013. C.V.M.
acknowledges HST Theory Grant HST-AR-13918.002-A. J.J.F. acknowledges
Hubble grants HST-GO-13501.06-A and HST-GO-13665.004-A and NSF grant
AST-1312545. M.S.M. acknowledges support of the NASA Origins program.
M.R.L. acknowledges support provided by NASA through Hubble Fellowship
grant #51362 awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
In., for NASA, under the contract NAS 5-26555.
NR 96
TC 15
Z9 15
U1 3
U2 12
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 DEC 20
PY 2015
VL 815
IS 2
AR 110
DI 10.1088/0004-637X/815/2/110
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300030
ER
PT J
AU Parker, DSN
Yang, T
Dangi, BB
Kaiser, RI
Bera, PP
Lee, TJ
AF Parker, Dorian S. N.
Yang, Tao
Dangi, Beni B.
Kaiser, Ralf. I.
Bera, Partha P.
Lee, Timothy J.
TI LOW TEMPERATURE FORMATION OF NITROGEN-SUBSTITUTED POLYCYCLIC AROMATIC
HYDROCARBONS (PANHs)-BARRIERLESS ROUTES TO DIHYDRO(iso)QUINOLINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; ISM: molecules; molecular processes
ID SINGLE-COLLISION CONDITIONS; CROSSED MOLECULAR-BEAM;
INTERSTELLAR-MEDIUM; AB-INITIO; EXTRATERRESTRIAL NUCLEOBASES;
CIRCUMSTELLAR ENVELOPES; MURCHISON METEORITE; CHEMICAL-DYNAMICS; ATOMIC
CARBON; PAH FORMATION
AB Meteorites contain bio-relevant molecules such as vitamins and nucleobases, which consist of aromatic structures with embedded nitrogen atoms. Questions remain over the chemical mechanisms responsible for the formation of nitrogen-substituted polycyclic aromatic hydrocarbons (PANHs) in extraterrestrial environments. By exploiting single collision conditions, we show that a radical mediated bimolecular collision between pyridyl radicals and 1,3-butadiene in the gas phase forms nitrogen-substituted polycyclic aromatic hydrocarbons (PANHs) 1,4-dihydroquinoline and to a minor amount 1,4-dihydroisoquinoline. The reaction proceeds through the formation of a van der Waals complex, which circumnavigates the entrance barrier implying it can operate at very low kinetic energy and therefore at low temperatures of 10 K as present in cold molecular clouds such as TMC-1. The discovery of facile de facto barrierless exoergic reaction mechanisms leading to PANH formation could play an important role in providing a population of aromatic structures upon which further photo-processing of ice condensates could occur to form nucleobases.
C1 [Parker, Dorian S. N.; Yang, Tao; Dangi, Beni B.; Kaiser, Ralf. I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Bera, Partha P.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Parker, DSN (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012
FU Department of Energy, Basic Energy Sciences [DE-FG02-03ER15411]; NASA
Postdoctoral Program; National Aeronautics and Space Administration
through the NASA Astrobiology Institute through the Science Mission
Directorate [NNH13ZDA017C]
FX The experimental work was supported by the Department of Energy, Basic
Energy Sciences (DE-FG02-03ER15411) at the University of Hawaii
(R.I.K.). This research was also supported by a Postdoctoral Fellow
Appointment by the NASA Postdoctoral Program (D.S.N.P.) administered by
Oak Ridge Associated Universities through a contract with NASA. The
computations are based upon work supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice NNH13ZDA017C issued through the Science
Mission Directorate. Computational work was performed using the Pleiades
supercomputer of the NASA Advanced Supercomputing Division, and our
in-house computers. The authors would like to thank Prof. Alexander
Mebel for sharing his RRKM code.
NR 69
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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 DEC 20
PY 2015
VL 815
IS 2
AR 115
DI 10.1088/0004-637X/815/2/115
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300035
ER
PT J
AU Ugarte-Urra, I
Upton, L
Warren, HP
Hathaway, DH
AF Ugarte-Urra, Ignacio
Upton, Lisa
Warren, Harry P.
Hathaway, David H.
TI MAGNETIC FLUX TRANSPORT AND THE LONG-TERM EVOLUTION OF SOLAR ACTIVE
REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: evolution; Sun: magnetic fields; Sun: photosphere;
Sun: UV radiation
ID DYNAMICS-OBSERVATORY SDO; MICHELSON DOPPLER IMAGER; MERIDIONAL FLOW;
SUN; FIELD; SURFACE; CYCLE; MAGNETOGRAMS; PARAMETERS; PLASMA
AB With multiple vantage points around the Sun, Solar Terrestrial Relations Observatory (STEREO) and Solar Dynamics Observatory imaging observations provide a unique opportunity to view the solar surface continuously. We use He II 304 angstrom data from these observatories to isolate and track ten active regions and study their long-term evolution. We find that active regions typically follow a standard pattern of emergence over several days followed by a slower decay that is proportional in time to the peak intensity in the region. Since STEREO does not make direct observations of the magnetic field, we employ a flux-luminosity relationship to infer the total unsigned magnetic flux evolution. To investigate this magnetic flux decay over several rotations we use a surface flux transport model, the Advective Flux Transport model, that simulates convective flows using a time-varying velocity field and find that the model provides realistic predictions when information about the active region's magnetic field strength and distribution at peak flux is available. Finally, we illustrate how 304 A images can be used as a proxy for magnetic flux measurements when magnetic field data is not accessible.
C1 [Ugarte-Urra, Ignacio] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Warren, Harry P.] Naval Res Lab, Div Space Sci, Code 7681, Washington, DC 20375 USA.
[Hathaway, David H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ugarte-Urra, I (reprint author), George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA.
OI Ugarte-Urra, Ignacio/0000-0001-5503-0491; Hathaway,
David/0000-0003-1191-3748; Warren, Harry/0000-0001-6102-6851
FU NASA [NNX13AE06G]
FX We would like to thank the referee for insightful comments that helped
improve the paper. I.U.U. acknowledges funding from the NASA grant
NNX13AE06G. H.P.W.'s participation was supported by CNR. The SECCHI data
are produced by an international consortium of the NRL, LMSAL and NASA
GSFC (USA), RAL and U. Bham (UK), MPS (Germany), CSL (Belgium), IOTA and
IAS (France). AIA and HMI data are courtesy of NASA/SDO and the AIA and
HMI science teams. I.U.U. and H.P.W. would like to thank Neil Sheeley
for many helpful conversations. I.U.U. also acknowledges useful comments
from William T. Thompson about the EUVI-AIA corrections available in the
Solar Soft STEREO beacon directories.
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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 DEC 20
PY 2015
VL 815
IS 2
AR 90
DI 10.1088/0004-637X/815/2/90
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300010
ER
PT J
AU Wang, J
Fischer, DA
Barclay, T
Picard, A
Ma, B
Bowler, BP
Schmitt, JR
Boyajian, TS
Jek, KJ
LaCourse, D
Baranec, C
Riddle, R
Law, NM
Lintott, C
Schawinski, K
Simister, DJ
Gregoire, B
Babin, SP
Poile, T
Jacobs, TL
Jebson, T
Omohundro, MR
Schwengeler, HM
Sejpka, J
Terentev, IA
Gagliano, R
Paakkonen, JP
Berge, HKO
Winarski, T
Green, GR
Schmitt, AR
Kristiansen, MH
Hoekstra, A
AF Wang, Ji
Fischer, Debra A.
Barclay, Thomas
Picard, Alyssa
Ma, Bo
Bowler, Brendan P.
Schmitt, Joseph R.
Boyajian, Tabetha S.
Jek, Kian J.
LaCourse, Daryll
Baranec, Christoph
Riddle, Reed
Law, Nicholas M.
Lintott, Chris
Schawinski, Kevin
Simister, Dean Joseph
Gregoire, Boscher
Babin, Sean P.
Poile, Trevor
Jacobs, Thomas Lee
Jebson, Tony
Omohundro, Mark R.
Schwengeler, Hans Martin
Sejpka, Johann
Terentev, Ivan A.
Gagliano, Robert
Paakkonen, Jari-Pekka
Berge, Hans Kristian Otnes
Winarski, Troy
Green, Gerald R.
Schmitt, Allan R.
Kristiansen, Martti H.
Hoekstra, Abe
TI PLANET HUNTERS. VIII. CHARACTERIZATION OF 41 LONG-PERIOD EXOPLANET
CANDIDATES FROM KEPLER ARCHIVAL DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; techniques: high angular resolution; techniques:
spectroscopic
ID TRANSIT TIMING VARIATIONS; ADAPTIVE OPTICS SYSTEM; EXTRASOLAR PLANETS;
STELLAR COMPANIONS; HABITABLE ZONE; GIANT PLANETS; LIGHT CURVES; SIZE
PLANET; HOST STARS; VALIDATION
AB The census of exoplanets is incomplete for orbital distances larger than 1 AU. Here, we present 41. long-period planet candidates in 38. systems identified by Planet Hunters based on Kepler archival data (Q0-Q17). Among them, 17. exhibit only one transit, 14. have two visible transits, and 10. have more than three visible transits. For planet candidates with only one visible transit, we estimate their orbital periods based on transit duration and host star properties. The majority of the planet candidates in this work (75%) have orbital periods that correspond to distances of 1-3 AU from their host stars. We conduct follow-up imaging and spectroscopic observations to validate and characterize planet host stars. In total, we obtain adaptive optics images for 33. stars to search for possible blending sources. Six stars have stellar companions within 4 ''. We obtain high-resolution spectra for 6. stars to determine their physical properties. Stellar properties for other stars are obtained from the NASA Exoplanet Archive and the Kepler Stellar Catalog by Huber et al. We validate 7 planet candidates that have planet confidence over 0.997 (3 sigma level). These validated planets include 3 single-transit planets (KIC-3558849b, KIC-5951458b, and KIC-8540376c), 3 planets with double transits (KIC-8540376b, KIC-9663113b, and KIC-10525077b), and 1 planet with four transits (KIC-5437945b). This work provides assessment regarding the existence of planets at wide separations and the associated false positive rate for transiting observation (17%-33%). More than half of the long-period planets with at least three transits in this paper exhibit transit timing variations up to 41 hr, which suggest additional components that dynamically interact with the transiting planet candidates. The nature of these components can be determined by follow-up radial velocity and transit observations.
C1 [Wang, Ji; Fischer, Debra A.; Picard, Alyssa; Schmitt, Joseph R.; Boyajian, Tabetha S.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Wang, Ji; Bowler, Brendan P.; Riddle, Reed] CALTECH, Pasadena, CA 91101 USA.
[Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Ma, Bo] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bowler, Brendan P.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA.
[Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Lintott, Chris] Oxford Astrophys, Oxford OX1 3RH, England.
[Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Kristiansen, Martti H.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
OI Schmitt, Joseph/0000-0003-1874-0552; Schawinski,
Kevin/0000-0001-5464-0888; Wang, Ji/0000-0002-4361-8885
FU National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt.
Cuba Astronomical Foundation; Alfred P. Sloan Foundation; Swiss National
Science Foundation [PP00P2_138979/1]; W. M. Keck Foundation; National
Aeronautics and Space Administration; NASA [NNX12AC01G, NNX15AF02G]
FX The authors would like to thank the anonymous referee whose comments and
suggestions greatly improve the paper. We are grateful to telescope
operators and supporting astronomers at the Palomar Observatory and the
Keck Observatory. 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
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. The research is made possible by the data from
the Kepler Community Follow-up Observing Program (CFOP). The authors
acknowledge all the CFOP users who uploaded the AO and RV data used in
the paper. We thank Katherine M. Deck for insightful comments on TTV
systems and the dynamical stability of KIC-10460629. 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. J.W., D.F. and T.B. acknowledge the support from NASA under
Grant No. NNX12AC01G and NNX15AF02G.; The Robo-AO system was developed
by collaborating partner institutions, the California Institute of
Technology and the Inter-University Centre for Astronomy and
Astrophysics, and with the support of the National Science Foundation
under Grant No. AST-0906060, AST-0960343 and AST-1207891, the Mt. Cuba
Astronomical Foundation and by a gift from Samuel Oschin. C.B.
acknowledges support from the Alfred P. Sloan Foundation. K.S.
gratefully acknowledges support from Swiss National Science Foundation
Grant PP00P2_138979/1.
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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 DEC 20
PY 2015
VL 815
IS 2
AR 127
DI 10.1088/0004-637X/815/2/127
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300047
ER
PT J
AU Zhang, S
Hailey, CJ
Mori, K
Clavel, M
Terrier, R
Ponti, G
Goldwurm, A
Bauer, FE
Boggs, SE
Christensen, FE
Craig, WW
Harrison, FA
Hong, J
Nynka, M
Soldi, S
Stern, D
Tomsick, JA
Zhang, WW
AF Zhang, Shuo
Hailey, Charles J.
Mori, Kaya
Clavel, Maica
Terrier, Regis
Ponti, Gabriele
Goldwurm, Andrea
Bauer, Franz E.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Harrison, Fiona A.
Hong, Jaesub
Nynka, Melania
Soldi, Simona
Stern, Daniel
Tomsick, John A.
Zhang, William W.
TI HARD X-RAY MORPHOLOGICAL AND SPECTRAL STUDIES OF THE GALACTIC CENTER
MOLECULAR CLOUD SGR B2: CONSTRAINING PAST SGR A(star) FLARING ACTIVITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; ISM: clouds; X-rays: individual (Sgr B2); X-rays: ISM
ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; 6.4 KEV LINE; CENTER
REGION; STAR-FORMATION; COSMIC-RAYS; XMM-NEWTON; CHANDRA OBSERVATIONS;
NONTHERMAL EMISSION; BRIGHTEST FLARE
AB In 2013, NuSTAR observed the Sgr B2 region and for the first time resolved its hard X-ray emission on subarcminute scales. Two prominent features are detected above 10 keV:. a newly emerging cloud, G0.66-0.13, and the central 90 '' radius region containing two compact cores, Sgr B2(M) and Sgr B2(N), surrounded by diffuse emission. It is inconclusive whether the remaining level of Sgr. B2 emission is still decreasing or has reached a constant background level. A decreasing X-ray emission can be best explained by the X-ray reflection nebula scenario, where the cloud reprocesses a past giant outburst from Sgr A(star). In the X-ray reflection nebula (XRN) scenario, the 3-79 keV Sgr. B2 spectrum allows us to self-consistently test the XRN model using both the Fe K alpha line and the continuum emission. The peak luminosity of the past Sgr A(star) outburst is constrained to L3-79keV similar to 5 x 10(38) ergs s(-1). A newly discovered cloud feature, G0.66-0.13, shows different timing variability. We suggest that it could be a molecular clump located in the Sgr B2 envelope reflecting the same Sgr A(star) outburst. In contrast, if the Sgr. B2 X-ray emission has reached a constant background level, it would imply an origin of low-energy cosmic-ray (CR) proton bombardment. In this scenario, from the NuSTAR measurements we infer a CR ion power of dW/dt = (1 - 4) x 10(39) erg s(-1) and a CR ionization rate of zeta(H) = (6 - 10) x 10(-15) H-1 s(-1). measurements can become powerful tools to constrain the GC CR population.
C1 [Zhang, Shuo; Hailey, Charles J.; Mori, Kaya; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Clavel, Maica; Goldwurm, Andrea] CEA Saclay, Serv Astrophys, IRFU, DSM, F-91191 Gif Sur Yvette, France.
[Terrier, Regis; Goldwurm, Andrea; Soldi, Simona] Unite Mixte Rech Astroparticule & Cosmol, F-75205 Paris, France.
[Ponti, Gabriele] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Zhang, S (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM shuo@astro.columbia.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Clavel, Maica/0000-0003-0724-2742
FU NASA [NNG08FD60C]; ESA Member States; NASA Headquarters under the NASA
Earth and Space Science Fellowship Program [NNX13AM31]; CONICYT-Chile;
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative; EU Marie Curie Intra European fellowship
[FP-PEOPLE-2012-IEF-331095]; Bundesministerium fur Wirtschaft und
Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR) [FKZ 50
OR 1408]; Max Planck Society; CNES
FX 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 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). This
research has also made use of data obtained with XMM-Newton, an ESA
science mission with instruments and contribution directly funded by ESA
Member States and NASA. S.Z. is supported by NASA Headquarters under the
NASA Earth and Space Science Fellowship Program-Grant "NNX13AM31."
F.E.B. acknowledges support from CONICYT-Chile and the Ministry of
Economy, Development, and Tourism's Millennium Science Initiative. G.P.
acknowledges support via an EU Marie Curie Intra European fellowship
under contract no. FP-PEOPLE-2012-IEF-331095 and Bundesministerium fur
Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt
(BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. M.C., A.G., R.T.,
and S.S. acknowledge support by CNES.
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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 DEC 20
PY 2015
VL 815
IS 2
AR 132
DI 10.1088/0004-637X/815/2/132
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ5OG
UT WOS:000367151300052
ER
PT J
AU Mawji, E
Schlitzer, R
Dodas, EM
Abadie, C
Abouchami, W
Anderson, RF
Baars, O
Bakker, K
Baskaran, M
Bates, NR
Bluhm, K
Bowie, A
Bown, J
Boye, M
Boyle, EA
Branellec, P
Bruland, KW
Brzezinski, MA
Bucciarelli, E
Buesseler, K
Butler, E
Cai, PH
Cardinal, D
Casciotti, K
Chaves, J
Cheng, H
Chever, F
Church, TM
Colman, AS
Conway, TM
Croot, PL
Cutter, GA
de Baar, HJW
de Souza, GF
Dehairs, F
Deng, FF
Dieu, HT
Dulaquais, G
Echegoyen-Sanz, Y
Edwards, RL
Fahrbach, E
Fitzsimmons, J
Fleisher, M
Frank, M
Friedrich, J
Fripiat, F
Galer, SJG
Gamo, T
Solsona, EG
Gerringa, LJA
Godoy, JM
Gonzalez, S
Grossteffan, E
Hatta, M
Hayes, CT
Heller, MI
Henderson, G
Huang, KF
Jeandel, C
Jenkins, WJ
John, S
Kenna, TC
Klunder, M
Kretschmer, S
Kumamoto, Y
Laan, P
Labatut, M
Lacan, F
Lam, PJ
Lannuzel, D
le Moigne, F
Lechtenfeld, OJ
Lohan, MC
Lu, YB
Masque, P
McClain, CR
Measures, C
Middag, R
Moffett, J
Navidad, A
Nishioka, J
Noble, A
Obata, H
Ohnemus, DC
Owens, S
Planchon, F
Pradoux, C
Puigcorbe, V
Quay, P
Radic, A
Rehkamper, M
Remenyi, T
Rijkenberg, MJA
Rintoul, S
Robinson, LF
Roeske, T
Rosenberg, M
van der Loeff, MR
Ryabenko, E
Saito, MA
Roshan, S
Salt, L
Sarthou, G
Schauer, U
Scott, P
Sedwick, PN
Sha, LJ
Shiller, AM
Sigman, DM
Smethie, W
Smith, GJ
Sohrin, Y
Speich, S
Stichel, T
Stutsman, J
Swift, JH
Tagliabue, A
Thomas, A
Tsunogai, U
Twining, BS
van Aken, HM
van Heuven, S
van Ooijen, J
van Weerlee, E
Venchiarutti, C
Voelker, AHL
Wake, B
Warner, MJ
Woodward, EMS
Wu, JF
Wyatt, N
Yoshikawa, H
Zheng, XY
Xue, ZC
Zieringer, M
Zimmer, LA
AF Mawji, Edward
Schlitzer, Reiner
Dodas, Elena Masferrer
Abadie, Cyril
Abouchami, Wafa
Anderson, Robert F.
Baars, Oliver
Bakker, Karel
Baskaran, Mark
Bates, Nicholas R.
Bluhm, Katrin
Bowie, Andrew
Bown, Johann
Boye, Marie
Boyle, Edward A.
Branellec, Pierre
Bruland, Kenneth W.
Brzezinski, Mark A.
Bucciarelli, Eva
Buesseler, Ken
Butler, Edward
Cai, Pinghe
Cardinal, Damien
Casciotti, Karen
Chaves, Joaquin
Cheng, Hai
Chever, Fanny
Church, Thomas M.
Colman, Albert S.
Conway, Tim M.
Croot, Peter L.
Cutter, Gregory A.
de Baar, Hein J. W.
de Souza, Gregory F.
Dehairs, Frank
Deng, Feifei
Huong Thi Dieu
Dulaquais, Gabriel
Echegoyen-Sanz, Yolanda
Edwards, R. Lawrence
Fahrbach, Eberhard
Fitzsimmons, Jessica
Fleisher, Martin
Frank, Martin
Friedrich, Jana
Fripiat, Francois
Galer, Stephen J. G.
Gamo, Toshitaka
Solsona, Ester Garcia
Gerringa, Loes J. A.
Godoy, Jose Marcus
Gonzalez, Santiago
Grossteffan, Emilie
Hatta, Mariko
Hayes, Christopher T.
Heller, Maija Iris
Henderson, Gideon
Huang, Kuo-Fang
Jeandel, Catherine
Jenkins, William J.
John, Seth
Kenna, Timothy C.
Klunder, Maarten
Kretschmer, Sven
Kumamoto, Yuichiro
Laan, Patrick
Labatut, Marie
Lacan, Francois
Lam, Phoebe J.
Lannuzel, Delphine
le Moigne, Frederique
Lechtenfeld, Oliver J.
Lohan, Maeve C.
Lu, Yanbin
Masque, Pere
McClain, Charles R.
Measures, Christopher
Middag, Rob
Moffett, James
Navidad, Alicia
Nishioka, Jun
Noble, Abigail
Obata, Hajime
Ohnemus, Daniel C.
Owens, Stephanie
Planchon, Frederic
Pradoux, Catherine
Puigcorbe, Viena
Quay, Paul
Radic, Amandine
Rehkaemper, Mark
Remenyi, Tomas
Rijkenberg, Micha J. A.
Rintoul, Stephen
Robinson, Laura F.
Roeske, Tobias
Rosenberg, Mark
van der Loeff, Michiel Rutgers
Ryabenko, Evgenia
Saito, Mak A.
Roshan, Saeed
Salt, Lesley
Sarthou, Geraldine
Schauer, Ursula
Scott, Peter
Sedwick, Peter N.
Sha, Lijuan
Shiller, Alan M.
Sigman, Daniel M.
Smethie, William
Smith, Geoffrey J.
Sohrin, Yoshiki
Speich, Sabrina
Stichel, Torben
Stutsman, Johnny
Swift, James H.
Tagliabue, Alessandro
Thomas, Alexander
Tsunogai, Urumu
Twining, Benjamin S.
van Aken, Hendrik M.
van Heuven, Steven
van Ooijen, Jan
van Weerlee, Evaline
Venchiarutti, Celia
Voelker, Antje H. L.
Wake, Bronwyn
Warner, Mark J.
Woodward, E. Malcolm S.
Wu, Jingfeng
Wyatt, Neil
Yoshikawa, Hisayuki
Zheng, Xin-Yuan
Xue, Zichen
Zieringer, Moritz
Zimmer, Louise A.
TI The GEOTRACES Intermediate Data Product 2014
SO MARINE CHEMISTRY
LA English
DT Article
DE GEOTRACES; Trace elements; Isotopes; Electronic atlas
AB The GEOTRACES Intermediate Data Product 2014 (IDP2014) is the first publicly available data product of the international GEOTRACES programme, and contains data measured and quality controlled before the end of 2013. It consists of two parts: (1) a compilation of digital data for more than 200 trace elements and isotopes (TEls) as well as classical hydrographic parameters, and (2) the eGEOTRACES Electronic Atlas providing a strongly inter-linked on-line atlas including more than 300 section plots and 90 animated 3D scenes. The IDP2014 covers the Atlantic, Arctic, and Indian oceans, exhibiting highest data density in the Atlantic. The TEI data in the IDP2014 are quality controlled by careful assessment of intercalibration results and multi-laboratory data comparisons at cross-over stations. The digital data are provided in several formats, including ASCII spreadsheet, Excel spreadsheet, netCDF, and Ocean Data View collection. In addition to the actual data values the IDP2014 also contains data quality flags and 1-sigma data error values where available. Quality flags and error values are useful for data filtering. Metadata about data originators, analytical methods and original publications related to the data are linked to the data in an easily accessible way. The eGEOTRACES Electronic Atlas is the visual representation of the IDP2014 data providing section plots and a new kind of animated 3D scenes. The basin-wide 3D scenes allow for viewing of data from many cruises at the same time, thereby providing quick overviews of large-scale tracer distributions. In addition, the 3D scenes provide geographical and bathymetric context that is crucial for the interpretation and assessment of observed tracer plumes, as well as for making inferences about controlling processes. (C) 2015 The Authors. Published by Elsevier B.V.
C1 [Mawji, Edward] Univ Southampton, British Oceanog Data Ctr, Southampton S014 3ZH, Hants, England.
[Schlitzer, Reiner; Fahrbach, Eberhard; Kretschmer, Sven; Lechtenfeld, Oliver J.; Roeske, Tobias; van der Loeff, Michiel Rutgers; Schauer, Ursula; Venchiarutti, Celia] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, D-27570 Bremerhaven, Germany.
[Dodas, Elena Masferrer; Abadie, Cyril; Jeandel, Catherine; Labatut, Marie; Lacan, Francois; Pradoux, Catherine; Radic, Amandine] Univ Toulouse 3, CNRS, CNES, IRD,LEGOS,, F-31400 Toulouse, France.
[Abouchami, Wafa; Galer, Stephen J. G.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Anderson, Robert F.; Fleisher, Martin; Hayes, Christopher T.; Kenna, Timothy C.; Smethie, William] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Baars, Oliver; Sigman, Daniel M.] MJ Univ, Dept Geosci, Princeton, NJ 08544 USA.
[Bakker, Karel; de Baar, Hein J. W.; Gerringa, Loes J. A.; Gonzalez, Santiago; Klunder, Maarten; Laan, Patrick; Rijkenberg, Micha J. A.; Salt, Lesley; van Aken, Hendrik M.; van Ooijen, Jan; van Weerlee, Evaline] Royal Netherlands Inst Sea Res, NL-1790 AB Den Burg, Netherlands.
[Baskaran, Mark] Wayne State Univ, Dept Geol, Detroit, MI 48202 USA.
[Bates, Nicholas R.] Bermuda Inst Ocean Sci, GE-01 St Georges, Bermuda.
[Bluhm, Katrin; Frank, Martin; Ryabenko, Evgenia; Zieringer, Moritz] Helmholtz Ctr Ocean Res Kiel, GEOMAR, D-24148 Kiel, Germany.
[Bowie, Andrew; Lannuzel, Delphine; Remenyi, Tomas] Univ Tasmania, Antarctic Climate & Ecosyst CRC, Hobart, Tas 7001, Australia.
[Bowie, Andrew; Lannuzel, Delphine; Remenyi, Tomas] Univ Tasmania, Inst Marine & Antarctic Studies, Hobart, Tas 7001, Australia.
[Bown, Johann; Boye, Marie; Dulaquais, Gabriel; Grossteffan, Emilie; Sarthou, Geraldine; Wake, Bronwyn] IUEM, IFREMER, CNRS, Lab Marine Environm Sci,LEMAR,UMR 6539,UBO,IRD, F-29280 Plouzane, France.
[Boyle, Edward A.; Echegoyen-Sanz, Yolanda; Fitzsimmons, Jessica] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Branellec, Pierre] IFREMER, F-29280 Plouzane, France.
[Bruland, Kenneth W.; Heller, Maija Iris; Lam, Phoebe J.; Smith, Geoffrey J.] Univ Calif Santa Cruz, Dept Ocean Sci, Santa Cruz, CA 95064 USA.
[Brzezinski, Mark A.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
[Brzezinski, Mark A.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Bucciarelli, Eva; Planchon, Frederic] Univ Brest, Lab Sci Environm Marin LEMAR, F-29280 Plouzane, France.
[Buesseler, Ken; Casciotti, Karen; Jenkins, William J.; Owens, Stephanie; Saito, Mak A.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA.
[Butler, Edward] Australian Inst Marine Sci, Casuarina, NT 0811, Australia.
[Cai, Pinghe] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen 361005, Peoples R China.
[Cardinal, Damien] Univ Paris 06, Univ Sorbonne, CNRS, IRD,MNHN,LOCEAN Lab, F-75252 Paris 5, France.
[Chaves, Joaquin; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Lab, Greenbelt, MD 20771 USA.
[Cheng, Hai; Sha, Lijuan] Xi An Jiao Tong Univ, Inst Global Environm Change, Xian 710049, Peoples R China.
[Chever, Fanny] Univ Southampton, Natl Oceanog Ctr, Sch Ocean & Earth Sci, Southampton S014 3ZH, Hants, England.
[Church, Thomas M.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Colman, Albert S.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Conway, Tim M.; John, Seth] Univ S Carolina, Dept Earth & Ocean Sci, Columbia, SC 29208 USA.
[Croot, Peter L.; Nishioka, Jun] Natl Univ Ireland Galway NU1 Galway, Sch Nat Sci, Dept Earth & Ocean Sci, Galway, Ireland.
[Cutter, Gregory A.; Sedwick, Peter N.; Zimmer, Louise A.] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA 23529 USA.
[de Souza, Gregory F.] Swiss Fed Inst Technol, Inst Geochem & Petrol, CH-8092 Zurich, Switzerland.
[Dehairs, Frank; Fripiat, Francois] Vrije Univ Brussel, Analyt Environm & Geochem Dept, B-1050 Brussels, Belgium.
[Deng, Feifei; Henderson, Gideon; Scott, Peter; Zheng, Xin-Yuan] Univ Oxford, Dept Earth Sci, Oxford 0X1 3AN, England.
[Huong Thi Dieu; Sohrin, Yoshiki] Kyoto Univ, Inst Chem Res, Uji 6110011, Japan.
[Edwards, R. Lawrence; Lu, Yanbin] Univ Minnesota, Dept Earth Sci, Minneapolis, MN 55455 USA.
[Friedrich, Jana] Helmholtz Zentrum Geesthacht, Ctr Mat & Coastal Res, D-21502 Geesthacht, Germany.
[Gamo, Toshitaka; Obata, Hajime] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778564, Japan.
[Solsona, Ester Garcia; Masque, Pere; Puigcorbe, Viena] Univ Autonoma Barcelona, Dept Phys, Bellaterra 08193, Spain.
[Solsona, Ester Garcia; Masque, Pere; Puigcorbe, Viena] Univ Autonoma Barcelona, Inst Environm Sci & Technol, Bellaterra 08193, Spain.
[Friedrich, Jana] Pontificia Univ Catolica Rio de Janeiro, Dept Chem, BR-22453900 Rio De Janeiro, Brazil.
[Hatta, Mariko; Measures, Christopher] Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA.
[Huang, Kuo-Fang] Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan.
[Kumamoto, Yuichiro] Japan Agcy Marine Earth Sci & Technol, Res & Dev Ctr Global Change, Yokosuka, Kanagawa 2370061, Japan.
[Rosenberg, Mark] Antarctic Climate & Ecosyst CRC, Hobart, Tas 7001, Australia.
[le Moigne, Frederique] Natl Oceanog Ctr, Southampton S014 3ZH, Hants, England.
[Lohan, Maeve C.; Wyatt, Neil] Univ Plymouth, Sch Geog Earth & Environm Sci, Drake Circus, Plymouth PLA 8AA, Devon, England.
[Middag, Rob] Univ Otago, Res Ctr Oceanog, NIWA, Dept Chem, Dunedin 9054, New Zealand.
[Moffett, James] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
CSIRO Marine & Atmospher Res, Hobart, Tas 7000, Australia.
Hokkaido Univ, Inst Low Temp Sci, Kita Ku, Sapporo, Hokkaido 0600819, Japan.
[Noble, Abigail] Environm Chem Grp, Cambridge, MA 02138 USA.
[Ohnemus, Daniel C.; Twining, Benjamin S.] Bigelow Lab Ocean Sci, East Boothbay, ME 04544 USA.
[Quay, Paul; Stutsman, Johnny; Warner, Mark J.] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Rehkaemper, Mark; Xue, Zichen] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England.
[Rintoul, Stephen] CSIRO Oceans & Atmosphere Flagship, Hobart, Tas 7001, Australia.
[Robinson, Laura F.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Shiller, Alan M.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA.
[Speich, Sabrina] Univ Western Brittany, Ocean Phys Lab, F-29285 Brest, France.
[Stichel, Torben] Univ Southampton, Natl Oceanog Ctr Southampton, Ocean & Earth Sci, Southampton S014 3ZH, Hants, England.
[Swift, James H.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Tagliabue, Alessandro] Univ Liverpool, Sch Environm Sci, Dept Earth Ocean & Ecol Sci, Liverpool L69 3BX, Merseyside, England.
[Thomas, Alexander] Univ Edinburgh, Sch Geosci, Grant Inst, Edinburgh EH9 3FE, Midlothian, Scotland.
[Tsunogai, Urumu] Nagoya Univ, Grad Sch Environm Studies, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[van Heuven, Steven] Univ Groningen, Energy & Sustainabil Res Inst Groningen, NL-9747 AG Groningen, Netherlands.
[Voelker, Antje H. L.] Portuguese Inst Ocean & Atmosphere IPMA, P-1449006 Lisbon, Portugal.
[Woodward, E. Malcolm S.] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Roshan, Saeed; Wu, Jingfeng] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, MAC, Miami, FL 33149 USA.
[Yoshikawa, Hisayuki] Hokkaido Univ, Grad Sch Environm Sci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yoshikawa, Hisayuki] Hokkaido Univ, Fac Environm Earth Sci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
RP Schlitzer, R (reprint author), Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Handelshafen 12, D-27570 Bremerhaven, Germany.
EM Reiner.Schlitzer@awi.de
RI Cutter, Gregory/C-7898-2017; Lacan, Francois/B-8032-2009; Croot,
Peter/C-8460-2009; Masque, Pere/B-7379-2008; Puigcorbe,
Viena/I-9349-2016; Shi, Wei/G-5129-2011; Tsunogai, Urumu/C-8303-2011;
Hayes, Christopher/P-3145-2016; Lechtenfeld, Oliver/A-6480-2013;
Voelker, Antje/C-5427-2012; Nishioka, Jun/F-5314-2011;
OI Cutter, Gregory/0000-0001-6744-6718; Croot, Peter/0000-0003-1396-0601;
Ohnemus, Daniel/0000-0001-6362-4134; Masque, Pere/0000-0002-1789-320X;
Puigcorbe, Viena/0000-0001-5892-2305; Robinson,
Laura/0000-0001-6811-0140; Tsunogai, Urumu/0000-0002-1517-3284; Hayes,
Christopher/0000-0002-5636-2989; Lechtenfeld,
Oliver/0000-0001-5313-6014; Voelker, Antje/0000-0001-6465-6023;
Baskaran, Mark/0000-0002-2218-4328; Zheng, Xin-Yuan/0000-0002-7959-8046;
Shiller, Alan/0000-0002-2068-7909; Lohan, Maeve/0000-0002-5340-3108;
Anderson, Robert/0000-0002-8472-2494; Wake, Bronwyn/0000-0002-9053-1264
FU Scientific Committee on Oceanic Research (SCOR) through grants from the
U.S. National Science Foundation [OCE-0608600, OCE-0938349,
OCE-1243377]; UK Natural Environment Research Council; Ministry of Earth
Science of India; Centre National de Recherche Scientifique,
l'Universite Paul Sabatier de Toulouse; Observatoire Midi-Pyrenees
Toulouse; Universitat Autonoma de Barcelona; Kiel Excellence Cluster The
Future Ocean; Swedish Museum of Natural History; University of Tokyo;
University of British Columbia; Royal Netherlands Institute for Sea
Research; GEOMAR-Helmholtz Centre for Ocean Research Kiel; Alfred
Wegener Institute
FX We gratefully acknowledge financial support by the Scientific Committee
on Oceanic Research (SCOR) through grants from the U.S. National Science
Foundation, including grants OCE-0608600, OCE-0938349, and OCE-1243377.
Financial support was also provided by the UK Natural Environment
Research Council, the Ministry of Earth Science of India, the Centre
National de Recherche Scientifique, l'Universite Paul Sabatier de
Toulouse, the Observatoire Midi-Pyrenees Toulouse, the Universitat
Autonoma de Barcelona, the Kiel Excellence Cluster The Future Ocean, the
Swedish Museum of Natural History, The University of Tokyo, The
University of British Columbia, The Royal Netherlands Institute for Sea
Research, the GEOMAR-Helmholtz Centre for Ocean Research Kiel, and the
Alfred Wegener Institute. This work is dedicated to the memory of
Eberhard Fahrbach, a great polar scientist and colleague whose legacy in
polar oceanography will carry on for the years to come. Eberhard served
as chief scientist on GIPY5 and was a long-time supporter of GEOTRACES.
NR 6
TC 25
Z9 25
U1 20
U2 67
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-4203
EI 1872-7581
J9 MAR CHEM
JI Mar. Chem.
PD DEC 20
PY 2015
VL 177
SI SI
BP 1
EP 8
DI 10.1016/j.marchem.2015.04.005
PN 1
PG 8
WC Chemistry, Multidisciplinary; Oceanography
SC Chemistry; Oceanography
GA CZ0IL
UT WOS:000366788300001
ER
PT J
AU Brown, LE
Chen, CY
Voytek, MA
Amirbahman, A
AF Brown, Lauren E.
Chen, Celia Y.
Voytek, Mary A.
Amirbahman, Aria
TI The effect of sediment mixing on mercury dynamics in two intertidal
mudflats at Great Bay Estuary, New Hampshire, USA
SO MARINE CHEMISTRY
LA English
DT Article
DE Mercury; Methylmercury; Sediment; Estuary
ID DISSOLVED ORGANIC-MATTER; PENOBSCOT RIVER ESTUARY; MARINE-SEDIMENTS;
METHYL MERCURY; METHYLMERCURY PRODUCTION; REDUCING BACTERIA; SURFACE
SEDIMENTS; NATURAL-WATERS; BOSTON HARBOR; PORE-WATER
AB Estuarine sediments store particulate contaminants including mercury (Hg). We studied Hg sediment dynamics in two intertidal mudflats at Great Bay estuary, NH, over multiple years. Sediments at both mudflats were physically mixed down to similar to 10 cm, as determined by Be-7 measurements, albeit via different mechanisms. Portsmouth mudflat (PT) sediments were subject to bioturbation by infaunal organisms and Squamscott mudflat (SQ) sediments were subject to erosion and redeposition. The presence of higher concentrations of fresh Fe(III) hydroxide at PT suggested bioirrigation by the polychaetes (Nereis virens). At depths where infaunal bioirrigation was observed, pore-water inorganic Hg (Hg-i) and methylmerculy (MeHg) were lower potentially due to their interaction with Fe(III) hydroxide. Methylmercury concentrations increased immediately below this zone in some samples, suggesting that the observed increase in material flux in bioirrigated sediments may initiate from lower depths. Pore water in sediment at PT also had higher fractions of more protein-like and labile DOC than those at SQ that can lead to increased MeHg production in PT, especially at depths where Hg, is not removed from solution by Fe(III) hydroxide. Where sediment erosion and redeposition were observed at SQ Hg species distribution was extended deeper into the sediment column. Moreover, methyl coenzyme M reductase (MCR) and mercury reductase (mer-A) genes were higher at SQthan PT suggesting differences in conditions for Hg cycling. Results showed that the near-surface region of high MeHg concentrations commonly observed in unmixed sediments does not exist in physically mixed sediments that are common in many estuarine environments. (C) 2015 Elsevier BM. All rights reserved.
C1 [Brown, Lauren E.; Amirbahman, Aria] Univ Maine, Dept Civil & Environm Engn, Orono, ME 04469 USA.
[Chen, Celia Y.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA.
[Voytek, Mary A.] NASA, Astrobiol Program, Washington, DC 20546 USA.
RP Amirbahman, A (reprint author), Univ Maine, Dept Civil & Environm Engn, Orono, ME 04469 USA.
EM ariaa@maine.edu
FU New Hampshire Sea Grant [R/CE-139]; NIH from the National Institute of
Environmental Health Sciences [P42 ES007373]
FX Funding for this work was provided by the New Hampshire Sea Grant,
project number: R/CE-139, and NIH Grant Number P42 ES007373 from the
National Institute of Environmental Health Sciences. Deenie Bugge, Julie
Kirshtein, Elizabeth Phillips, Michael Swett, and Vivien Taylor are
acknowledged for their assistance. Three anonymous reviewers provided
valuable critiques of the manuscript.
NR 82
TC 0
Z9 0
U1 5
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-4203
EI 1872-7581
J9 MAR CHEM
JI Mar. Chem.
PD DEC 20
PY 2015
VL 177
BP 731
EP 741
DI 10.1016/j.marchem.2015.10.011
PN 5
PG 11
WC Chemistry, Multidisciplinary; Oceanography
SC Chemistry; Oceanography
GA CZ0IT
UT WOS:000366789100006
PM 26924879
ER
PT J
AU Sinha, PR
Gupta, P
Kaskaoutis, DG
Sahu, LK
Nagendra, N
Manchanda, RK
Kumar, YB
Sreenivasan, S
AF Sinha, P. R.
Gupta, Pawan
Kaskaoutis, D. G.
Sahu, L. K.
Nagendra, N.
Manchanda, R. K.
Kumar, Y. B.
Sreenivasan, S.
TI Estimation of particulate matter from satellite- and ground-based
observations over Hyderabad, India
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; URBAN STATION HYDERABAD; LONG-RANGE TRANSPORT;
AIR-QUALITY; LEVEL PM2.5; SUN PHOTOMETER; BLACK CARBON; ARABIAN SEA;
MODIS; VARIABILITY
AB Long-term trends in surface-level particulate matter of dynamic diameter 2 mu m (PM2) in regard to air quality observations over Greater Hyderabad Region (GHR), India are estimated by the synergy of ground-based measurements and satellite observations during the period 2001-2013 (satellite) and July 2009-Dec 2013 (ground-based). Terra Moderate Resolution Imaging Spectroradiometer (MODIS)-derived aerosol optical thickness (AOT) (MODIS-AOTs) was validated against that measured from Microtops-II Sunphotometer (MTS) AOTs (MTS-AOTs) and then utilized to estimate surface-level PM2 concentrations over GHR using regression analysis between MODIS-AOTs, MTS-AOTs, and measured PM2. In general, the MODIS-estimated PM2 concentrations fell within the uncertainty of the measurements, thus allowing the estimate of PM2 from MODIS, although in some cases they differed significantly due to vertical heterogeneity in aerosol distribution and the presence of distinct elevated aerosol layers of different origin and characteristics. Furthermore, significant spatial and temporal heterogeneity in the AOT and PM2 estimates is observed in urban environments, especially during the pre-monsoon and monsoon seasons, which reduces the accuracy of the PM2 estimates from MODIS. The estimates of PM2 using MTS or MODIS-AOT exhibit a root mean square deference (RMSD) of about 8-16% against measured PM2 on a seasonal basis. Furthermore, a tendency of increasing PM2 concentrations is observed, which however is difficult to quantify for urban areas due to uncertainties in PM2 estimations and gaps in the data set. Examination of surface and columnar aerosol concentrations, along with meteorological parameters from radiosonde observations on certain days, reveals that changes in local emissions and boundary-layer dynamics, and the presence or arrival of distinct aerosol plumes aloft, are major concerns in the accurate estimation of PM2 from MODIS, while the large spatial distribution of aerosol and pollutants in the urban environment makes such estimates a considerable challenge.
C1 [Sinha, P. R.; Nagendra, N.; Manchanda, R. K.; Sreenivasan, S.] Tata Inst Fundamental Res, Balloon Facil, Hyderabad 500062, Andhra Pradesh, India.
[Sinha, P. R.] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Sinha, P. R.] Natl Inst Polar Res, Tachikawa, Tokyo, Japan.
[Gupta, Pawan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Gupta, Pawan] Univ Space Res Assoc, Greenbelt, MD 20770 USA.
[Kaskaoutis, D. G.] Shiv Nadar Univ, Sch Nat Sci, Dept Phys, Dadri 203207, Ncr, India.
[Sahu, L. K.] Phys Res Lab, Space & Atmospher Sci Div, Ahmadabad 380009, Gujarat, India.
[Manchanda, R. K.] Univ Mumbai, Dept Phys, Bombay 400098, Maharashtra, India.
[Kumar, Y. B.] Natl Atmospher Res Lab, Gadanki 517112, India.
RP Sinha, PR (reprint author), Tata Inst Fundamental Res, Balloon Facil, Hyderabad 500062, Andhra Pradesh, India.
EM prs@tifr.res.in
RI Yellapragada, Bhavani Kumar/G-1228-2010
OI Yellapragada, Bhavani Kumar/0000-0001-7462-6223
FU ISRO-HQ Bengaluru under ISRO-GBP-ARFI
FX The authors wish to thank ISRO-HQ Bengaluru for financial support under
ISRO-GBP-ARFI.
NR 48
TC 3
Z9 3
U1 3
U2 13
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD DEC 20
PY 2015
VL 36
IS 24
BP 6192
EP 6213
DI 10.1080/01431161.2015.1112929
PG 22
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA CX7FI
UT WOS:000365867200010
ER
PT J
AU Massaro, F
Thompson, D
Ferrara, E
AF Massaro, Francesco
Thompson, David J.
Ferrara, Elizabeth C.
TI The extragalactic gamma-ray sky in the Fermi era
SO ASTRONOMY AND ASTROPHYSICS REVIEW
LA English
DT Review
DE Gamma rays; Extragalactic astronomy; Active galactic nuclei; Quasars; BL
Lac objects; Background light
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; INTERGALACTIC
MAGNETIC-FIELD; SPECTRUM RADIO-SOURCES; BL LACERTAE OBJECTS; LINE
SEYFERT 1; LOG-PARABOLIC SPECTRA; QUASAR 3C 454.3; LAC OBJECTS; SOURCE
CATALOG
AB The Universe is largely transparent to -rays in the GeV energy range, making these high-energy photons valuable for exploring energetic processes in the cosmos. After 7 years of operation, the Fermi Gamma-ray Space Telescope has produced a wealth of information about the high-energy sky. This review focuses on extragalactic -ray sources: what has been learned about the sources themselves and about how they can be used as cosmological probes. Active galactic nuclei (blazars, radio galaxies, Seyfert galaxies) and star-forming galaxies populate the extragalactic high-energy sky. Fermi observations have demonstrated that these powerful non-thermal sources display substantial diversity in energy spectra and temporal behavior. Coupled with contemporaneous multifrequency observations, the Fermi results are enabling detailed, time-dependent modeling of the energetic particle acceleration and interaction processes that produce the -rays, as well as providing indirect measurements of the extragalactic background light and intergalactic magnetic fields. Population studies of the -ray source classes compared to the extragalactic -ray background place constraints on some models of dark matter. Ongoing searches for the nature of the large number of -ray sources without obvious counterparts at other wavelengths remain an important challenge.
C1 [Massaro, Francesco] Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy.
[Thompson, David J.; Ferrara, Elizabeth C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Massaro, F (reprint author), Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy.
EM fmassaro@stanford.edu; david.j.thompson@nasa.gov;
elizabeth.c.ferrara@nasa.gov
RI Massaro, Francesco/L-9102-2016
OI Massaro, Francesco/0000-0002-1704-9850
FU Programma Giovani Ricercatori-Rita Levi Montalcini-Rientro dei Cervelli;
NASA [NNX12AO97G, NNX13AP20G]; National Aeronautics and Space
Administration
FX This review would not have been possible without the dedicated efforts
of scientists, engineers, and technicians who have made the Fermi
Gamma-ray Space Telescope mission so successful. We extend thanks to all
those who contributed. Special thanks to Justin Finke, Filippo D'Ammando
and Seth Digel for valuable comments on the manuscript. F. Massaro
wishes to thank M. Ajello, R. D'Abrusco, D. Gasparrini, M. Giroletti, L.
Latronico, N. Masetti, A. Paggi, H. Smith and G. Tosti for their support
during the last 4 years spent working on Fermi blazars. The work by is
supported by the Programma Giovani Ricercatori-Rita Levi
Montalcini-Rientro dei Cervelli (2012). This review is also supported by
the NASA grants NNX12AO97G and NNX13AP20G. Part of this work is based on
archival data, software or on-line services provided by the ASI Science
Data Center. This research has made use of data obtained from the
high-energy Astrophysics Science Archive Research Center (HEASARC)
provided by NASA's Goddard Space Flight Center; the SIMBAD database
operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic
Database (NED) operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. This publication makes use of data products
from 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. TOPCAT
(http://www.star.bris.ac.uk/similar to mbt/topcat/) (Taylor 2005) for
the preparation and manipulation of the tabular data and the images. The
Aladin Java applet (http://aladin.u-strasbg.fr/aladin.gml) was used to
create the finding charts reported in this paper (Bonnarel 2000). It can
be started from the CDS (Strasbourg, France), from the CFA (Harvard,
USA), from the ADAC (Tokyo, Japan), from the IUCAA (Pune, India), from
the UKADC (Cambridge, UK), or from the CADC (Victoria, Canada).
NR 262
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0935-4956
EI 1432-0754
J9 ASTRON ASTROPHYS REV
JI Astron. Astrophys. Rev.
PD DEC 19
PY 2015
VL 24
BP 1
EP 58
DI 10.1007/s00159-015-0090-6
PG 58
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ3LD
UT WOS:000367004700001
ER
PT J
AU Rivero-Calle, S
Gnanadesikan, A
Del Castillo, CE
Balch, WM
Guikema, SD
AF Rivero-Calle, Sara
Gnanadesikan, Anand
Del Castillo, Carlos E.
Balch, William M.
Guikema, Seth D.
TI Multidecadal increase in North Atlantic coccolithophores and the
potential role of rising CO2
SO SCIENCE
LA English
DT Article
ID OCEAN ACIDIFICATION; EMILIANIA-HUXLEYI; ATMOSPHERIC CO2; CARBON FLUXES;
PHYTOPLANKTON; CALCIFICATION; PATTERNS
AB As anthropogenic carbon dioxide (CO2) emissions acidify the oceans, calcifiers generally are expected to be negatively affected. However, using data from the Continuous Plankton Recorder, we show that coccolithophore occurrence in the North Atlantic increased from similar to 2 to more than 20% from 1965 through 2010. We used random forest models to examine more than 20 possible environmental drivers of this change, finding that CO2 and the Atlantic Multidecadal Oscillation were the best predictors, leading us to hypothesize that higher CO2 levels might be encouraging growth. A compilation of 41 independent laboratory studies supports our hypothesis. Our study shows a long-term basin-scale increase in coccolithophores and suggests that increasing CO2 and temperature have accelerated the growth of a phytoplankton group that is important for carbon cycling.
C1 [Rivero-Calle, Sara; Gnanadesikan, Anand; Del Castillo, Carlos E.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Rivero-Calle, Sara] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
[Del Castillo, Carlos E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Balch, William M.] Bigelow Lab Ocean Sci, East Boothbay, ME USA.
[Guikema, Seth D.] Univ Michigan, Dept Ind & Operat Engn, Ann Arbor, MI 48109 USA.
RP Rivero-Calle, S (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM sara.rivero@jhu.edu; gnanades@jhu.edu
RI Gnanadesikan, Anand/A-2397-2008; Del Castillo, Carlos/N-2601-2013
OI Gnanadesikan, Anand/0000-0001-5784-1116;
FU Johns Hopkins University; Applied Physics Laboratory; NSF (Division of
Ocean Sciences); NASA (Ocean Biology and Biogeochemistry Program);
[NSF-1149460]
FX We thank D. Johns, the Sir Alister Hardy for Ocean Science (SAHFOS)
Associated External Researcher fund, and everyone involved in the CPR
survey. We thank the Johns Hopkins University and the Applied Physics
Laboratory for financial support and B. Zaitchik, D. Waugh, J. Dunne,
and three anonymous reviewers for helpful comments. Funding for S.D.G.
was from NSF-1149460. Support for W.B. came from NSF (Division of Ocean
Sciences) and NASA (Ocean Biology and Biogeochemistry Program). CPR data
used in this study can be obtained from SAHFOS upon request.
NR 24
TC 12
Z9 12
U1 16
U2 73
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 DEC 18
PY 2015
VL 350
IS 6267
BP 1533
EP 1537
DI 10.1126/science.aaa8026
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CY7LY
UT WOS:000366591100060
PM 26612836
ER
PT J
AU Takada, M
Dore, O
AF Takada, Masahiro
Dore, Olivier
TI Geometrical constraint on curvature with BAO experiments
SO PHYSICAL REVIEW D
LA English
DT Article
ID BARYON ACOUSTIC-OSCILLATIONS; MICROWAVE BACKGROUND ANISOTROPY; DIGITAL
SKY SURVEY; COSMOLOGICAL CONSTANT; OPEN UNIVERSE; GALAXIES; DISTANCE;
SCALE; INFLATION; VACUUM
AB The spatial curvature (K or Omega(K)) is one of the most fundamental parameters of an isotropic and homogeneous universe and has a close link to the physics of the early Universe. Combining the radial and angular diameter distances measured via the baryon acoustic oscillation (BAO) experiments allows us to unambiguously constrain the curvature. The method is primarily based on the metric theory, and is less sensitive to the theory of structure formation (other than the existence of the BAO scale) and is free of any model of dark energy. In this paper, we estimate a best achievable accuracy of constraining the curvature with the BAO experiments. We show that an all-sky, cosmic-variance-limited galaxy survey covering the Universe up to z greater than or similar to 4 enables a precise determination of the curvature to an accuracy of sigma(Omega(K)) similar or equal to 10(-3). When we assume a model of dark energy-either the cosmological constraint or the (w(0), w(a)) model-it can achieve a precision of sigma(Omega(K)) similar or equal to a few x 10(-4). These forecasts require a high sampling density of galaxies, and are degraded by up to a factor of a few for a survey with a finite number density of similar to 10(-3) (h/Mpc)(3).
C1 [Takada, Masahiro] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, Inst Adv Study, WPI, Chiba 2778583, Japan.
[Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Takada, M (reprint author), Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, Inst Adv Study, WPI, Chiba 2778583, Japan.
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; FIRST program Subaru Measurements of Images and Redshifts
(SuMIRe), CSTP, Japan; MEXT [15H05893, 15K21733]; JSPS Promotion of
Science [23340061, 26610058]; JSPS Program for Advancing Strategic
International Networks to Accelerate the Circulation of Talented
Researchers; National Science Foundation [PHYS-1066293]
FX We thank Gary Bernstein, Neal Dalal, Chris Hirata, Eiichiro Komatsu,
Hitoshi Murayama, Yasunori Nomura, Hirosi Ooguri, and Misao Sasaki for
useful discussion. M. T. is supported by the World Premier International
Research Center Initiative (WPI Initiative), MEXT, Japan, by the FIRST
program Subaru Measurements of Images and Redshifts (SuMIRe), CSTP,
Japan, by a MEXT Grant-in-Aid for Scientific Research on Innovative
Areas, "Why does the Universe accelerate?-Exhaustive study and challenge
for the future -" (No. 15H05893 and No. 15K21733), by a Grant-in-Aid for
Scientific Research from the JSPS Promotion of Science (No. 23340061 and
No. 26610058), and by the JSPS Program for Advancing Strategic
International Networks to Accelerate the Circulation of Talented
Researchers. 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. O. D. thanks IPMU for its generous hospitality. This
work is also supported in part by the National Science Foundation under
Grant No. PHYS-1066293 and the hospitality of the Aspen Center for
Physics.
NR 57
TC 5
Z9 5
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD DEC 17
PY 2015
VL 92
IS 12
AR 123518
DI 10.1103/PhysRevD.92.123518
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CY9NQ
UT WOS:000366734000002
ER
PT J
AU Chronis, T
Lang, T
Koshak, W
Blakeslee, R
Christian, H
McCaul, E
Bailey, J
AF Chronis, T.
Lang, T.
Koshak, W.
Blakeslee, R.
Christian, H.
McCaul, E.
Bailey, J.
TI Diurnal characteristics of lightning flashes detected over the Sao Paulo
lightning mapping array
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MESOSCALE CONVECTIVE SYSTEM; UNITED-STATES; THUNDERSTORM
ELECTRIFICATION; FLORIDA THUNDERSTORMS; SOUTHEASTERN BRAZIL;
PEAK-CURRENT; CHARGE; CYCLE; WEATHER; CLOUDS
AB This study examines diurnal variations of lightning flash characteristics observed by the Lightning Mapping Array in Sao Paulo, Brazil. The diurnal flash counts exhibit the typical afternoon convective maximum. The mean source altitude demonstrates a discrete increase that is temporally coincident with the local sunrise. The mean horizontal and vertical flash extents each attain a maximum (minimum) around local sunrise (afternoon, i.e., 13:00-17:00 local solar time). In addition, joint histograms of flash horizontal and vertical extents show that the majority of the flashes occurring during the afternoon convection are shorter and more comparable in size, and the differences between the horizontal and vertical extents are reduced. Conversely, flashes preceding and following the peak in afternoon convection are less symmetric, with larger horizontal than vertical extents. We discuss whether these observations could be partially explained by the diurnal variations in the convectively induced mixing regimes that control thundercloud charge regions and associated charge separation distances. The documented diurnal flash characteristics closely match recently published findings on the diurnal variation of the peak currents of cloud-to-ground flashes. Possible physical mechanisms for these observations are discussed.
C1 [Chronis, T.; Christian, H.; Bailey, J.] Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
[Lang, T.; Koshak, W.; Blakeslee, R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[McCaul, E.] Univ Space Res Assoc, Huntsville, AL USA.
RP Chronis, T (reprint author), Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
EM themis.chronis@nsstc.uah.edu
OI Lang, Timothy/0000-0003-1576-572X
FU GOES-R System Program as part of Proving Ground and Risk Reduction
programs
FX The first author acknowledges the support by Steve Goodman and the
GOES-R System Program as part of the Proving Ground and Risk Reduction
programs. The authors would also like to extend their appreciation to
Ken Cummins for the insightful comments. The CHUVA data can be freely
accessed at
http://chuvaproject.cptec.inpe.br/portal/noticia.ultimas.logic. This
paper has been greatly improved by the constructive suggestions of
anonymous reviewers.
NR 50
TC 2
Z9 2
U1 5
U2 7
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD023960
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700001
ER
PT J
AU Koukouli, ME
Lerot, C
Granville, J
Goutail, F
Lambert, JC
Pommereau, JP
Balis, D
Zyrichidou, I
Van Roozendael, M
Coldewey-Egbers, M
Loyola, D
Labow, G
Frith, S
Spurr, R
Zehner, C
AF Koukouli, M. E.
Lerot, C.
Granville, J.
Goutail, F.
Lambert, J. -C.
Pommereau, J. -P.
Balis, D.
Zyrichidou, I.
Van Roozendael, M.
Coldewey-Egbers, M.
Loyola, D.
Labow, G.
Frith, S.
Spurr, R.
Zehner, C.
TI Evaluating a new homogeneous total ozone climate data record from
GOME/ERS-2, SCIAMACHY/Envisat, and GOME-2/MetOp-A
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; TEMPERATURE-DEPENDENCE;
SATELLITE-OBSERVATIONS; SENSORS GOME/ERS-2; UV SPECTROSCOPY; COLUMN
OZONE; BREWER; DOBSON; GOME; SPECTROPHOTOMETERS
AB The European Space Agency's Ozone Climate Change Initiative (O-3-CCI) project aims at producing and validating a number of high-quality ozone data products generated from different satellite sensors. For total ozone, the O-3-CCI approach consists of minimizing sources of bias and systematic uncertainties by applying a common retrieval algorithm to all level 1 data sets, in order to enhance the consistency between the level 2 data sets from individual sensors. Here we present the evaluation of the total ozone products from the European sensors Global Ozone Monitoring Experiment (GOME)/ERS-2, SCIAMACHY/Envisat, and GOME-2/MetOp-A produced with the GOME-type Direct FITting (GODFIT) algorithm v3. Measurements from the three sensors span more than 16 years, from 1996 to 2012. In this work, we present the latest O-3-CCI total ozone validation results using as reference ground-based measurements from Brewer and Dobson spectrophotometers archived at the World Ozone and UV Data Centre of the World Meteorological Organization as well as from UV-visible differential optical absorption spectroscopy (DOAS)/Systeme D'Analyse par Observations Zenithales (SAOZ) instruments from the Network for the Detection of Atmospheric Composition Change. In particular, we investigate possible dependencies in these new GODFIT v3 total ozone data sets with respect to latitude, season, solar zenith angle, and different cloud parameters, using the most adequate type of ground-based instrument. We show that these three O-3-CCI total ozone data products behave very similarly and are less sensitive to instrumental degradation, mainly as a result of the new reflectance soft-calibration scheme. The mean bias to the ground-based observations is found to be within the 1 +/- 1% level for all three sensors while the near-zero decadal stability of the total ozone columns (TOCs) provided by the three European instruments falls well within the 1-3% requirement of the European Space Agency's Ozone Climate Change Initiative project.
C1 [Koukouli, M. E.; Balis, D.; Zyrichidou, I.] Aristotle Univ Thessaloniki, Lab Atmospher Phys, GR-54006 Thessaloniki, Greece.
[Lerot, C.; Granville, J.; Lambert, J. -C.; Van Roozendael, M.] Belgian Inst Space Aeron, Brussels, Belgium.
[Goutail, F.; Pommereau, J. -P.] Versailles St Quentin En Yvelines Univ, CNRS, LATMOS, Guyancourt, France.
[Coldewey-Egbers, M.; Loyola, D.] German Aerosp Ctr, Remote Sensing Technol Inst, Wessling, Germany.
[Labow, G.; Frith, S.] Sci Syst & Applicat Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Spurr, R.] RT Solut Inc, Cambridge, MA USA.
[Zehner, C.] ESA ESRIN, Frascati, Italy.
RP Koukouli, ME (reprint author), Aristotle Univ Thessaloniki, Lab Atmospher Phys, GR-54006 Thessaloniki, Greece.
EM mariliza@auth.gr
FU ESA's Climate Change Initiative - Ozone project; Belgian Federal Science
Policy Office (BelSPO); ProDEx via A3C project
FX The authors are grateful to ESA's Climate Change Initiative - Ozone
project for providing the funding necessary of this work. Part of this
work has also been funded by the Belgian Federal Science Policy Office
(BelSPO) and ProDEx via the A3C project. The ground-based data used in
this publication were obtained as part of WMO's Global Atmosphere Watch
(GAW) and the Network for the Detection of Atmospheric Composition
Change (NDACC). They are publicly available via the World Ozone and UV
Data Centre (WOUDC) and the NDACC Data Host Facility (see
http://woudc.org and http://ndacc.org, respectively). We would like to
acknowledge and warmly thank all the investigators that provide data to
these repositories on a timely basis, as well as the handlers of these
databases for their upkeep and quality guaranteed efforts.
NR 58
TC 3
Z9 3
U1 0
U2 5
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD023699
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700033
ER
PT J
AU Mazrooei, A
Sinha, T
Sankarasubramanian, A
Kumar, S
Peters-Lidard, CD
AF Mazrooei, Amirhossein
Sinha, Tushar
Sankarasubramanian, A.
Kumar, Sujay
Peters-Lidard, Christa D.
TI Decomposition of sources of errors in seasonal streamflow forecasting
over the US Sunbelt
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RAINFALL-RUNOFF REGIME; WESTERN UNITED-STATES; COMMUNITY LAND MODEL;
SOIL-MOISTURE; CLIMATE MODELS; RIVER-BASIN; PRECIPITATION; PREDICTION;
SYSTEM; PREDICTABILITY
AB Seasonal streamflow forecasts, contingent on climate information, can be utilized to ensure water supply for multiple uses including municipal demands, hydroelectric power generation, and for planning agricultural operations. However, uncertainties in the streamflow forecasts pose significant challenges in their utilization in real-time operations. In this study, we systematically decompose various sources of errors in developing seasonal streamflow forecasts from two Land Surface Models (LSMs) (Noah3.2 and CLM2), which are forced with downscaled and disaggregated climate forecasts. In particular, the study quantifies the relative contributions of the sources of errors from LSMs, climate forecasts, and downscaling/disaggregation techniques in developing seasonal streamflow forecast. For this purpose, three month ahead seasonal precipitation forecasts from the ECHAM4.5 general circulation model (GCM) were statistically downscaled from 2.8 degrees to 1/8 degrees spatial resolution using principal component regression (PCR) and then temporally disaggregated from monthly to daily time step using kernel-nearest neighbor (K-NN) approach. For other climatic forcings, excluding precipitation, we considered the North American Land Data Assimilation System version 2 (NLDAS-2) hourly climatology over the years 1979 to 2010. Then the selected LSMs were forced with precipitation forecasts and NLDAS-2 hourly climatology to develop retrospective seasonal streamflow forecasts over a period of 20 years (1991-2010). Finally, the performance of LSMs in forecasting streamflow under different schemes was analyzed to quantify the relative contribution of various sources of errors in developing seasonal streamflow forecast. Our results indicate that the most dominant source of errors during winter and fall seasons is the errors due to ECHAM4.5 precipitation forecasts, while temporal disaggregation scheme contributes to maximum errors during summer season.
C1 [Mazrooei, Amirhossein; Sankarasubramanian, A.] N Carolina State Univ, Dept Civil Construct & Environm Engn, Raleigh, NC 27695 USA.
[Sinha, Tushar] Texas A&M Univ, Dept Environm Engn, Kingsville, TX USA.
[Kumar, Sujay; Peters-Lidard, Christa D.] Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD USA.
RP Mazrooei, A (reprint author), N Carolina State Univ, Dept Civil Construct & Environm Engn, Raleigh, NC 27695 USA.
EM amazroo@ncsu.edu
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NC Water Resources Research Institute (NC-WRRI); NASA
FX All the data used from the study could be obtained by from USGS, NASA,
and IRI library. Data from decomposition experiments could be obtained
by contacting the authors. The first author's Masters thesis research
was partially supported by the NC Water Resources Research Institute
(NC-WRRI). Any opinions, findings, and conclusions or recommendations
expressed in this paper are those of the authors and do not reflect the
views of the NC-WRRI. All data related to this manuscript could be
obtained from Amirhossein Mazrooei (amazroo@ncsu.edu).
NR 45
TC 1
Z9 1
U1 1
U2 4
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD023687
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700002
ER
PT J
AU Rezac, L
Jian, Y
Yue, J
Russell, JM
Kutepov, A
Garcia, R
Walker, K
Bernath, P
AF Rezac, L.
Jian, Y.
Yue, J.
Russell, J. M., III
Kutepov, A.
Garcia, R.
Walker, K.
Bernath, P.
TI Validation of the global distribution of CO2 volume mixing ratio in the
mesosphere and lower thermosphere from SABER
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ACCELERATED LAMBDA ITERATION; CARBON-DIOXIDE; RADIATIVE-TRANSFER; MIDDLE
ATMOSPHERE; MU-M; EXCITATION; EMISSION; SPECTROMETER; ABUNDANCES;
RADIANCES
AB The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics satellite has been measuring the limb radiance in 10 broadband infrared channels over the altitude range from similar to 400 km to the Earth's surface since 2002. The kinetic temperatures and CO2 volume mixing ratios (VMRs) in the mesosphere and lower thermosphere have been simultaneously retrieved using SABER limb radiances at 15 and 4.3 mu m under nonlocal thermodynamic equilibrium (non-LTE) conditions. This paper presents results of a validation study of the SABER CO2 VMRs obtained with a two-channel, self-consistent temperature/CO2 retrieval algorithm. Results are based on comparisons with coincident CO2 measurements made by the Atmospheric Chemistry Experiment Fourier transform spectrometer (ACE-FTS) and simulations using the Specified Dynamics version of the Whole Atmosphere Community Climate Model (SD-WACCM). The SABER CO2 VMRs are in agreement with ACE-FTS observations within reported systematic uncertainties from 65 to 110 km. The annual average SABER CO2 VMR falls off from a well-mixed value above similar to 80 km. Latitudinal and seasonal variations of CO2 VMRs are substantial. SABER observations and the SD-WACCM simulations are in overall agreement for CO2 seasonal variations, as well as global distributions in the mesosphere and lower thermosphere. Not surprisingly, the CO2 seasonal variation is shown to be driven by the general circulation, converging in the summer polar mesopause region and diverging in the winter polar mesopause region.
C1 [Rezac, L.] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany.
[Rezac, L.; Jian, Y.; Yue, J.; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Kutepov, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kutepov, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Garcia, R.] Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA.
[Walker, K.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bernath, P.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA USA.
RP Rezac, L (reprint author), Max Planck Inst Sonnensyst Forsch, Gottingen, Germany.
EM rezac@mps.mpg.de
RI Yue, Jia/D-8177-2011; Bernath, Peter/B-6567-2012
OI Bernath, Peter/0000-0002-1255-396X
FU NASA Langley Research Center, NASA Goddard Space Flight Center, Spain
(IAA); Arcon, Inc.; NASA grant [NNX11AD63G, NNX14AF20G,
NNH13ZDA001N-HGI, NNX11AM24G]; Canadian Space Agency; U.S. National
Science Foundation
FX We would like to acknowledge the hard work and support of the SABER
retrieval team who provided the version 2.0 data, including scientists
from GATS, Inc, NASA Langley Research Center, NASA Goddard Space Flight
Center, Spain (IAA), and Arcon, Inc. The SABER experiment and retrieval
work are supported by NASA grant NNX11AD63G. The ACE mission is
supported primarily by the Canadian Space Agency. The National Center
for Atmospheric Research is supported by the U.S. National Science
Foundation. L.R. acknowledges funding from NASA grant NNX11AD63G. J.Y.
is supported by NASA grants NNX14AF20G and NNH13ZDA001N-HGI. A.K. was
supported by NASA grant NNX11AM24G. We are grateful to Martin Kaufmann
for providing the CRISTA CO2 profiles. The new v2.0 SABER
products as well as the simultaneously retrieved
Tk/CO2 presented in this paper are accessible from
the SABER website: http://saber.gats-inc.com/data.php. We thank the two
anonymous reviewers for their constructive comments, which improved this
manuscript.
NR 44
TC 2
Z9 2
U1 1
U2 8
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD023955
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700018
ER
PT J
AU Sayer, AM
Hsu, NC
Bettenhausen, C
Jeong, MJ
Meister, G
AF Sayer, A. M.
Hsu, N. C.
Bettenhausen, C.
Jeong, M-J.
Meister, G.
TI Effect of MODIS Terra radiometric calibration improvements on Collection
6 Deep Blue aerosol products: Validation and Terra/Aqua consistency
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RESOLUTION IMAGING SPECTRORADIOMETER; OPTICAL DEPTH RETRIEVALS;
REFLECTIVE SOLAR BANDS; ON-ORBIT CALIBRATION; DATA-ASSIMILATION; DIURNAL
VARIABILITY; SOURCE REGIONS; OCEAN; LAND; SATELLITE
AB The Deep Blue (DB) algorithm's primary data product is midvisible aerosol optical depth (AOD). DB applied to Moderate Resolution Imaging Spectroradiometer (MODIS) measurements provides a data record since early 2000 for MODIS Terra and mid-2002 for MODIS Aqua. In the previous data version (Collection 5, C5), DB production from Terra was halted in 2007 due to sensor degradation; the new Collection 6 (C6) has both improved science algorithms and sensor radiometric calibration. This includes additional calibration corrections developed by the Ocean Biology Processing Group to address MODIS Terra's gain, polarization sensitivity, and detector response versus scan angle, meaning DB can now be applied to the whole Terra record. Through validation with Aerosol Robotic Network (AERONET) data, it is shown that the C6 DB Terra AOD quality is stable throughout the mission to date. Compared to the C5 calibration, in recent years the RMS error compared to AERONET is smaller by similar to 0.04 over bright (e.g., desert) and similar to 0.01-0.02 over darker (e.g., vegetated) land surfaces, and the fraction of points in agreement with AERONET within expected retrieval uncertainty higher by similar to 10% and similar to 5%, respectively. Comparisons to the Aqua C6 time series reveal a high level of correspondence between the two MODIS DB data records, with a small positive (Terra-Aqua) average AOD offset < 0.01. The analysis demonstrates both the efficacy of the new radiometric calibration efforts and that the C6 MODIS Terra DB AOD data remain stable (to better than 0.01 AOD) throughout the mission to date, suitable for quantitative scientific analyses.
C1 [Sayer, A. M.; Hsu, N. C.; Bettenhausen, C.; Meister, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Sayer, A. M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Greenbelt, MD USA.
[Bettenhausen, C.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Jeong, M-J.] Gangneung Wonju Natl Univ, Kangnung, South Korea.
RP Sayer, AM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM andrew.sayer@nasa.gov
RI Sayer, Andrew/H-2314-2012
OI Sayer, Andrew/0000-0001-9149-1789
FU NASA EOS program; Development of Geostationary Meteorological Satellite
Ground Segment program - National Meteorological Satellite Centre of
Korea Meteorological Administration
FX This work was supported by the NASA EOS program, managed by H. Maring.
M.-J. Jeong was supported by the Development of Geostationary
Meteorological Satellite Ground Segment program funded by the National
Meteorological Satellite Centre of the Korea Meteorological
Administration. The authors gratefully acknowledge the AERONET site PIs
(C. J. Bruegge, B. Chatenet, H.-B. Chen, P. Goloub, B. N. Holben, A.
Karnieli, S. Khabba, C.M.B. Lehmann, D. Moore, B. Mougenot, S. Piketh,
A.M. Silva, R. Mitchell, R.P. Singh, D. Tanr, S.N. Tripathi, and G.
Zibordi), site managers, supporting institutions, and the AERONET team
for the creation and stewardship of the Sun-photometer data records. The
MODIS Characterization Support Team and Ocean Biology Processing Group
are thanked for their extensive efforts in maintaining the high
radiometric quality of MODIS data. AERONET data are available from
aeronet.gsfc.nasa.gov and MODIS data from ladsweb.nascom.nasa.gov. Three
anonymous reviewers are thanked for their helpful comments on this
manuscript.
NR 52
TC 6
Z9 6
U1 5
U2 13
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD023878
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700024
ER
PT J
AU Thorsen, TJ
Fu, Q
AF Thorsen, Tyler J.
Fu, Qiang
TI CALIPSO-inferred aerosol direct radiative effects: Bias estimates using
ground-based Raman lidars
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; CIRRUS CLOUDS; OPTICAL DEPTH;
SATELLITE-OBSERVATIONS; A-TRAIN; ACCURATE PARAMETERIZATION; TROPOSPHERIC
AEROSOLS; AUTOMATED RETRIEVAL; CLIMATE MODELS; EXTINCTION
AB Observational constraints on the change in the radiative energy budget caused by the presence of aerosols, i.e., the aerosol direct radiative effect (DRE), have recently been made using observations from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite (CALIPSO). CALIPSO observations have the potential to provide improved global estimates of aerosol DRE compared to passive sensor-derived estimates due to CALIPSO's ability to perform vertically resolved aerosol retrievals over all surface types and over cloud. In this study, uncertainties in CALIPSO-inferred aerosol DRE are estimated using multiple years of observations from the Atmospheric Radiation Measurement (ARM) program's Raman lidars at midlatitude and tropical sites. We find that CALIPSO is unable to detect all radiatively significant aerosol, resulting in an underestimate in the magnitude of the aerosol DRE by 30-50% at the two ARM sites. The undetected aerosol is likely the consequence of random noise in CALIPSO measurements and therefore will affect global observations as well. This suggests that the global aerosol DRE inferred from CALIPSO observations are likely too weak. Also examined is the impact of the ratio of extinction-to-backscatter (i.e., the lidar ratio) whose value CALIPSO retrievals must assume to obtain the aerosol extinction profile. It is shown that if CALIPSO can reproduce the climatological value of the lidar ratio at a given location, then the aerosol DRE there can be accurately calculated (within about 3%).
C1 [Thorsen, Tyler J.; Fu, Qiang] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Thorsen, Tyler J.] NASA, Langley Res Ctr, Postdoctoral Program, Hampton, VA 23665 USA.
RP Thorsen, TJ (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
EM tyler.thorsen@nasa.gov
FU Office of Science (BER) U.S. Department of Energy [DE-SC0010557]; NASA
[NNX13AN49G, NNX14AB28G]; NASA Postdoctoral Program Fellowship
FX The Raman lidar, radiosonde, and surface radiation data sets were
obtained from the ARM data archive: www.archive.arm.gov. The CALIPSO
data sets were obtained from the NASA Langley Research Center
Atmospheric Science Data Center. This research was supported by the
Office of Science (BER) U.S. Department of Energy grant DE-SC0010557 and
by NASA grants NNX13AN49G and NNX14AB28G. T.J. Thorsen was also
supported by a NASA Postdoctoral Program Fellowship.
NR 63
TC 4
Z9 4
U1 1
U2 9
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 DEC 16
PY 2015
VL 120
IS 23
DI 10.1002/2015JD024095
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB3PD
UT WOS:000368422700027
ER
PT J
AU Daly, EA
Brodeur, RD
AF Daly, Elizabeth A.
Brodeur, Richard D.
TI Warming Ocean Conditions Relate to Increased Trophic Requirements of
Threatened and Endangered Salmon
SO PLOS ONE
LA English
DT Article
ID COLUMBIA RIVER PLUME; NORTHERN CALIFORNIA CURRENT; EARLY MARINE
RESIDENCE; SPRING CHINOOK SALMON; PACIFIC SALMON; ONCORHYNCHUS-KISUTCH;
CLIMATE-CHANGE; SOCKEYE-SALMON; INTERDECADAL VARIABILITY;
FOOD-CONSUMPTION
AB The trophic habits, size and condition of yearling Chinook salmon (Oncorhynchus tshawytscha) caught early in their marine residence were examined during 19 survey years (1981-1985; 1998-2011). Juvenile salmon consumed distinct highly piscivorous diets in cold and warm ocean regimes with major differences between ocean regimes driven by changes in consumption of juvenile rockfishes, followed by several other fish prey, adult euphausiids and decapod larvae. Notable, Chinook salmon consumed 30% more food in the warm versus cold ocean regime in both May and June. Additionally, there were about 30% fewer empty stomachs in the warm ocean regime in May, and 10% fewer in warm June periods. The total prey energy density consumed during the warmer ocean regime was also significantly higher than in cold. Chinook salmon had lower condition factor and were smaller in fork length during the warm ocean regime, and were longer and heavier for their size during the cold ocean regime. The significant increase in foraging during the warm ocean regime occurred concurrently with lower available prey biomass. Adult return rates of juvenile Chinook salmon that entered the ocean during a warm ocean regime were lower. Notably, our long term data set contradicts the long held assertion that juvenile salmon eat less in a warm ocean regime when low growth and survival is observed, and when available prey are reduced. Comparing diet changes between decades under variable ocean conditions may assist us in understanding the effects of projected warming ocean regimes on juvenile Chinook salmon and their survival in the ocean environment. Bioenergetically, the salmon appear to require more food resources during warm ocean regimes.
C1 [Daly, Elizabeth A.] Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
[Brodeur, Richard D.] NOAA, Fish Ecol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR USA.
RP Daly, EA (reprint author), Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
EM Elizabeth.daly@oregonstate.edu
FU Bonneville Power Administration [1998-014-00]
FX This work was supported by the Bonneville Power Administration, project
#1998-014-00 (http://www.bpa.gov/).
NR 80
TC 4
Z9 4
U1 7
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 DEC 16
PY 2015
VL 10
IS 12
AR e0144066
DI 10.1371/journal.pone.0144066
PG 23
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CY9JH
UT WOS:000366722700023
PM 26675673
ER
PT J
AU Shalm, LK
Meyer-Scott, E
Christensen, BG
Bierhorst, P
Wayne, MA
Stevens, MJ
Gerrits, T
Glancy, S
Hamel, DR
Allman, MS
Coakley, KJ
Dyer, SD
Hodge, C
Lita, AE
Verma, VB
Lambrocco, C
Tortorici, E
Migdall, AL
Zhang, YB
Kumor, DR
Farr, WH
Marsili, F
Shaw, MD
Stern, JA
Abellan, C
Amaya, W
Pruneri, V
Jennewein, T
Mitchell, MW
Kwiat, PG
Bienfang, JC
Mirin, RP
Knill, E
Nam, SW
AF Shalm, Lynden K.
Meyer-Scott, Evan
Christensen, Bradley G.
Bierhorst, Peter
Wayne, Michael A.
Stevens, Martin J.
Gerrits, Thomas
Glancy, Scott
Hamel, Deny R.
Allman, Michael S.
Coakley, Kevin J.
Dyer, Shellee D.
Hodge, Carson
Lita, Adriana E.
Verma, Varun B.
Lambrocco, Camilla
Tortorici, Edward
Migdall, Alan L.
Zhang, Yanbao
Kumor, Daniel R.
Farr, William H.
Marsili, Francesco
Shaw, Matthew D.
Stern, Jeffrey A.
Abellan, Carlos
Amaya, Waldimar
Pruneri, Valerio
Jennewein, Thomas
Mitchell, Morgan W.
Kwiat, Paul G.
Bienfang, Joshua C.
Mirin, Richard P.
Knill, Emanuel
Nam, Sae Woo
TI Strong Loophole-Free Test of Local Realism
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID HIDDEN-VARIABLE THEORIES; BELL INEQUALITIES; SUGGESTED INTERPRETATION;
QUANTUM-THEORY; VIOLATION; MECHANICS; PHOTONS; THEOREM; TERMS
AB We present a loophole-free violation of local realism using entangled photon pairs. We ensure that all relevant events in our Bell test are spacelike separated by placing the parties far enough apart and by using fast random number generators and high-speed polarization measurements. A high-quality polarization-entangled source of photons, combined with high-efficiency, low-noise, single-photon detectors, allows us to make measurements without requiring any fair-sampling assumptions. Using a hypothesis test, we compute p values as small as 5.9 x 10(-9) for our Bell violation while maintaining the spacelike separation of our events. We estimate the degree to which a local realistic system could predict our measurement choices. Accounting for this predictability, our smallest adjusted p value is 2.3 x 10(-7). We therefore reject the hypothesis that local realism governs our experiment.
C1 [Shalm, Lynden K.; Bierhorst, Peter; Stevens, Martin J.; Gerrits, Thomas; Glancy, Scott; Allman, Michael S.; Coakley, Kevin J.; Dyer, Shellee D.; Hodge, Carson; Lita, Adriana E.; Verma, Varun B.; Lambrocco, Camilla; Tortorici, Edward; Mirin, Richard P.; Knill, Emanuel; Nam, Sae Woo] NIST, Boulder, CO 80305 USA.
[Meyer-Scott, Evan; Zhang, Yanbao; Jennewein, Thomas] Univ Waterloo, Inst Quantum Comp, Waterloo, ON N2L 3G1, Canada.
[Meyer-Scott, Evan; Zhang, Yanbao; Jennewein, Thomas] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Christensen, Bradley G.; Wayne, Michael A.; Kumor, Daniel R.; Kwiat, Paul G.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Wayne, Michael A.; Migdall, Alan L.; Bienfang, Joshua C.] NIST, Gaithersburg, MD 20899 USA.
[Hamel, Deny R.] Univ Moncton, Dept Phys & Astron, Moncton, NB E1A 3E9, Canada.
[Migdall, Alan L.; Bienfang, Joshua C.] NIST, Joint Quantum Inst, Gaithersburg, MD 20899 USA.
[Migdall, Alan L.; Bienfang, Joshua C.] Univ Maryland, Gaithersburg, MD 20899 USA.
[Farr, William H.; Marsili, Francesco; Shaw, Matthew D.; Stern, Jeffrey A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Abellan, Carlos; Amaya, Waldimar; Pruneri, Valerio; Mitchell, Morgan W.] Barcelona Inst Sci & Technol, ICFO Inst Ciencies Foton, Castelldefels 08860, Barcelona, Spain.
[Pruneri, Valerio; Mitchell, Morgan W.] ICREA, Barcelona 08015, Spain.
[Jennewein, Thomas] Canadian Inst Adv Res, Quantum Informat Sci Program, Toronto, ON, Canada.
RP Shalm, LK (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA.
RI Mitchell, Morgan/I-9027-2012; Hamel, Deny/C-7071-2017; Amaya Ocampo,
Waldimar/C-8667-2012; Abellan, Carlos/N-4561-2014
OI Mitchell, Morgan/0000-0001-8949-9407; Hamel, Deny/0000-0002-4788-7548;
BIERHORST, PETER/0000-0003-2781-5448; Amaya Ocampo,
Waldimar/0000-0002-6930-8914; Abellan, Carlos/0000-0003-1122-6622
FU DARPA; NIST Quantum Information Program; NSF [PHY 12-05870]; MURI Center
for Photonic Quantum Information Systems (ARO/ARDA Program)
[DAAD19-03-1-0199]; Office of Naval Research MURI on Fundamental
Research on Wavelength-Agile High-Rate Quantum Key Distribution (QKD) in
a Marine Environment [N00014-13-0627]; NSERC; CIFAR; Industry Canada;
NASA; European Research Council project AQUMET; European Union Project
QUIC [641122]; Spanish MINECO under the Severo Ochoa programme
[SEV-2015-0522]; project MAGO [FIS2011-23520]; project EPEC
[FIS2014-62181-EXP]; Catalan AGAUR SGR Grants [1295, 1623]; European
Regional Development Fund (FEDER) [TEC2013-46168-R]; Fundacio Privada
CELLEX; New Brunswick Innovation Foundation
FX We thank Todd Harvey for assistance with optical fiber installation;
Norman Sanford for the use of lab space; Kevin Silverman, Aephraim M.
Steinberg, Rupert Ursin, Marissa Giustina, Stephen Jordan, Dietrich
Leibfried, and Paul Lett for helpful discussions; Nik Luhrs and Kristina
Meier for help with the electronics; Andrew Novick for help with the GPS
measurements; Joseph Chapman and Malhar Jere for designing the cultural
pseudorandom numbers; and Stephen Jordan, Paul Lett, and Dietrich
Leibfried for constructive comments on the manuscript. We thank Conrad
Turner Bierhorst for waiting patiently for the computation of p values.
We acknowledge support for this project provided by DARPA (L. K. S., M.
S. A., A. E. L., S. D. D., M. J. S., V. B. V., T. G., R. P. M., S. W.
N., W. H. F., F. M., M. D. S., J. A. S.) and the NIST Quantum
Information Program (L. K. S., M. S. A., A. E. L., S. D. D., M. J. S.,
V. B. V., T. G., S. G., P. B., J. C. B., A. M., R. P. M., E. K., S. W.
N.); NSF Grant No. PHY 12-05870 and MURI Center for Photonic Quantum
Information Systems (ARO/ARDA Program DAAD19-03-1-0199) DARPA InPho
program and the Office of Naval Research MURI on Fundamental Research on
Wavelength-Agile High-Rate Quantum Key Distribution (QKD) in a Marine
Environment, Grant No. N00014-13-0627 (B. G. C., M. A. W., D. R. K., P.
G. K.); NSERC, CIFAR and Industry Canada (E. M. S., Y. Z., T. J.); NASA
(F. M., M. D. S., W. H. F., J. A. S.); European Research Council project
AQUMET, European Union Project QUIC (Grant Agreement No. 641122),
Spanish MINECO under the Severo Ochoa programme (Grant No.
SEV-2015-0522) and projects MAGO (Grant No. FIS2011-23520) and EPEC
(Grant No. FIS2014-62181-EXP), Catalan AGAUR 2014 SGR Grants No. 1295
and No. 1623, the European Regional Development Fund (FEDER) Grant No.
TEC2013-46168-R, and by Fundacio Privada CELLEX (M. W. M., C. A., W. A.,
V. P.); and New Brunswick Innovation Foundation (D. R. H.). Part of the
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 48
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Z9 95
U1 7
U2 27
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 DEC 16
PY 2015
VL 115
IS 25
AR 250402
DI 10.1103/PhysRevLett.115.250402
PG 10
WC Physics, Multidisciplinary
SC Physics
GA CY5ZL
UT WOS:000366486600002
PM 26722906
ER
PT J
AU Scoville, J
Sornette, J
Freund, FT
AF Scoville, John
Sornette, Jaufray
Freund, Friedemann T.
TI Paradox of peroxy defects and positive holes in rocks Part II: Outflow
of electric currents from stressed rocks
SO JOURNAL OF ASIAN EARTH SCIENCES
LA English
DT Article
DE Stress-activated currents; Peroxy defects; Positive holes; Outflow
currents; Pre-Earthquake processes
ID IGNEOUS ROCKS; EARTHQUAKE; CRUSTAL; TAIWAN; FAULT; FIELD; MGO
AB Understanding the electrical properties of rocks is of fundamental interest. We report on currents generated when stresses are applied. Loading the center of gabbro tiles, 30 x 30 x 0.9 cm(3), across a 5 cm diameter piston, leads to positive currents flowing from the center to the unstressed edges. Changing the constant rate of loading over 5 orders of magnitude from 0.2 kPa/s to 20 MPa/s produces positive currents, which start to flow already at low stress levels, <5 MPa. The currents increase as long as stresses increase. At constant load they flow for hours, days, even weeks and months, slowly decreasing with time. When stresses are removed, they rapidly disappear but can be made to reappear upon reloading. These currents are consistent with the stress-activation of peroxy defects, such as O3Si-OO-SiO3, in the matrix of rock-forming minerals. The peroxy break-up leads to positive holes h, i.e. electronic states associated with 0(-) in a matrix of 0(2-), plus electrons, e'. Propagating along the upper edge of the valence band, the h. are able to flow from stressed to unstressed rock, traveling fast and far by way of a phonon-assisted electron hopping mechanism using energy levels at the upper edge of the valence band. Impacting the tile center leads to h. pulses, 4-6 ms long, flowing outward at similar to 100 m/s at a current equivalent to 1-2 x 10(9) A/km(3). Electrons, trapped in the broken peroxy bonds, are also mobile, but only within the stressed volume. (c) 2015 The Authors. Published by Elsevier Ltd.
C1 [Scoville, John; Freund, Friedemann T.] GeoCosmo Sci & Res Ctr, Moffett Field, CA 94035 USA.
[Scoville, John; Freund, Friedemann T.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Scoville, John; Sornette, Jaufray] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freund, Friedemann T.] SETI Inst, Mountain View, CA 94043 USA.
[Freund, Friedemann T.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Freund, FT (reprint author), NASA, Ames Res Ctr, MS 245-4, Moffett Field, CA 94035 USA.
EM friedemann.t.freund@nasa.gov
FU GEST (Goddard Earth Science Technology) Fellowship; NASA Earth Surface
and Interior (ESI) program [NNX12AL71G]; iSTEP project
[NSC102-2628-M-008-001]
FX The early part of this work was supported through a GEST (Goddard Earth
Science Technology) Fellowship and later through a grant NNX12AL71G from
the NASA Earth Surface and Interior (ESI) program to Friedemann Freund.
We thank Professor Charles Schwartz, University of Maryland, Department
of Civil Engineering, for giving us the opportunity to use the hydraulic
press. We thank Lynn Hofland, NASA Ames Research Center, Engineering
Evaluation Laboratory (EEL), for his assistance during the drop tower
experiments. We thank AJ Udom for his participation as part of his NASA
Ames Summer 2013 Internship, and we thank Gary Cyr for help with setting
up the data acquisition system. The publication fee is supported by the
iSTEP project NSC102-2628-M-008-001.
NR 32
TC 5
Z9 5
U1 4
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1367-9120
EI 1878-5786
J9 J ASIAN EARTH SCI
JI J. Asian Earth Sci.
PD DEC 15
PY 2015
VL 114
SI SI
BP 338
EP 351
DI 10.1016/j.jseaes.2015.04.016
PN 2
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA DA5QN
UT WOS:000367857700008
ER
PT J
AU Freund, FT
Freund, MM
AF Freund, Friedemann T.
Freund, Minoru M.
TI Paradox of peroxy defects and positive holes in rocks. Part I: Effect of
temperature
SO JOURNAL OF ASIAN EARTH SCIENCES
LA English
DT Article
DE Electrical conductivity; Magnesium oxide; Peroxy defects; Positive hole
charge carriers; Thermal activation; Igneous rocks; High-grade
metamorphic rocks
ID ALKALINE-EARTH OXIDES; MAGNESIUM-OXIDE; ELECTRICAL-CONDUCTIVITY;
SINGLE-CRYSTAL; THERMAL-DECOMPOSITION; HIGH-PURITY; HYDROGEN; MGO;
ENERGY; CARBON
AB Most non-seismic, non-geodesic pre-earthquake phenomena are believed to be controlled by the stress-activation of peroxy defects in rocks, which release highly mobile electric charges. Though ubiquitous in minerals of igneous and high-grade metamorphic rocks, peroxy defects have been widely overlooked in the past. The charge carriers of interest are positive holes, chemically equivalent to O- in a matrix of O2-, physically defect electrons in the O2- sublattice, highly mobile, able to propagate fast and far. O- are oxidized relative to O2-. As such O- are not supposed to exist in minerals and rocks that come from deep within the Earth's crust, where the environments are overwhelmingly reduced. The presence of O- appears to contradict thermodynamics. However, there is no conflict. In order to understand how peroxy defects are introduced into common rock-forming minerals, over which temperature window they release positive holes, and how this may be related to pre-earthquake phenomena, we look at peroxy defects in a aystallographically and compositionally well characterized model system: single crystals of nominally high-purity MgO, grown from the melt under highly reducing conditions. During crystallization the MgO crystals incorporate OH- through dissolution of traces of H2O in the MgO matrix, leading to a solid solution ( ss ) Mg1-delta(OH)2(delta)O(1-2 delta), where delta << 1. During cooling, the ss leaves thermodynamic equilibrium, turning into a metastable supersaturated solid solution (sss). Using infrared (IR) spectroscopy it is shown that, during further cooling, OH- pairs at Mg2+ vacancy sites rearrange their electrons, undergoing a redox conversion, which leads to peroxy anions, O-2(2-), plus molecular H-2. Being diffusively mobile, the H-2 molecules can leave the Mg2+ vacancy sites, leaving behind cation-deficient Mg1-delta O. During reheating, but in the sss range, the O-2(2-) break up, releasing positive hole charge carriers, which profoundly affect the electrical conductivity behavior. In igneous mafic and ultramafic rocks, similar changes in the electrical conductivity are observed in the temperature window, where peroxy defects of the type 0(3)Si-00-SiO3 break up. They release positive holes, which control the electrical conductivity response. Deciphering these processes helps understanding the stress-activation of positive holes along the geotherm. (c) 2015 Published by Elsevier Ltd.. C 2015 Published by Elsevier Ltd.
C1 [Freund, Friedemann T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freund, Friedemann T.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Freund, Friedemann T.] SETI Inst, Boston, MA USA.
[Freund, Minoru M.] NASA, Ames Res Ctr, Ctr Nanotechnol & Adv Space Mat, Moffett Field, CA 94035 USA.
RP Freund, FT (reprint author), NASA, Ames Res Ctr, MS 245-4, Moffett Field, CA 94035 USA.
EM friedemann.t.freund@nasa.gov
FU Deutsche Forschungsgemeinschaft; NASA Ames Research Center Director's
Discretionary Fund; NASA Earth Surface and Interior (ESI) program
[NNX12AL71G]; iSTEP project [NSC102-2628-M-008-001]
FX The results reported in this paper evolved over many years, starting
with early studies by Reinhard Martens, Heinz Wengeler and Hendrik
Kathrein, supported in part by the Deutsche Forschungsgemeinschaft, and
continuing with work supported over several years by the NASA Ames
Research Center Director's Discretionary Fund and, most recently, by the
NASA Earth Surface and Interior (ESI) program under grant # NNX12AL71G.;
The publication fee is supported by the iSTEP project
NSC102-2628-M-008-001.
NR 48
TC 0
Z9 0
U1 3
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1367-9120
EI 1878-5786
J9 J ASIAN EARTH SCI
JI J. Asian Earth Sci.
PD DEC 15
PY 2015
VL 114
SI SI
BP 373
EP 383
DI 10.1016/j.jseaes.2015.04.047
PN 2
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DA5QN
UT WOS:000367857700011
ER
PT J
AU Gaillardin, M
Raine, M
Paillet, P
Adell, PC
Girard, S
Duhamel, O
Andrieu, F
Barraud, S
Faynot, O
AF Gaillardin, M.
Raine, M.
Paillet, P.
Adell, P. C.
Girard, S.
Duhamel, O.
Andrieu, F.
Barraud, S.
Faynot, O.
TI Investigations on heavy ion induced Single-Event Transients (SETs) in
highly-scaled FinFETs
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Single-Event Effect (SEE); FinFET; Heavy ion; Geant4; TCAD
ID ENERGY ELECTROMAGNETIC MODELS; GEANT4 PHYSICS PROCESSES; RADIATION
RESPONSE; MOS-TRANSISTORS; SOI MOSFETS; GATE; DEVICES; SILICON;
DEGRADATION; IRRADIATION
AB We investigate Single-Event Transients (SET) in different designs of multiple-gate devices made of FinFETs with various geometries. Heavy ion experimental results are explained by using a thorough charge collection analysis of fast transients measured on dedicated test structures. Multi-level simulations are performed to get new insights into the charge collection mechanisms in multiple-gate devices. Implications for multiple-gate device design hardening are finally discussed. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Gaillardin, M.; Raine, M.; Paillet, P.; Duhamel, O.] CEA, DAM, DIF, F-91297 Arpajon, France.
[Adell, P. C.] Jet Prop Lab, Pasadena, CA 91101 USA.
[Girard, S.] Univ St Etienne, Lab H Curien, UMR 5516, F-42000 St Etienne, France.
[Andrieu, F.; Barraud, S.; Faynot, O.] CEA, LETI Minatec, F-38000 Grenoble, France.
RP Gaillardin, M (reprint author), CEA, DAM, DIF, F-91297 Arpajon, France.
EM marc.gaillardin@cea.fr
FU NASA Electronic Part and Packaging
FX The authors would like to thanks the GANIL technical staff during heavy
ion tests and the CIRIL for providing the heavy ion beam time to perform
tests for this study. The authors also would like to thank the NASA
Electronic Part and Packaging for their support.
NR 27
TC 0
Z9 0
U1 5
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
EI 1872-9584
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD DEC 15
PY 2015
VL 365
BP 631
EP 635
DI 10.1016/j.nimb.2015.08.085
PN B
PG 5
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA CZ0HZ
UT WOS:000366787000037
ER
PT J
AU Xu, SS
Liemohn, MW
Peterson, WK
Fontenla, J
Chamberlin, P
AF Xu, Shaosui
Liemohn, Michael W.
Peterson, W. K.
Fontenla, Juan
Chamberlin, Phillip
TI Comparison of different solar irradiance models for the superthermal
electron transport model for Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Photoelectron; Solar irradiance models; Superthermal electron transport;
Mars
ID MARTIAN ATMOSPHERE; IONOSPHERE; PLASMASPHERE; EXPRESS; MISSION; FLUXES;
RATES; FIELD; WIND; EUV
AB As the solar photon fluxes directly control the production of photoelectrons, it is important to examine the influence of different solar irradiance models on the photoelectron fluxes. In this study, we present the implementation of the two recent solar irradiance models, the Flare Irradiance Spectral Model (FISM) and the Heliospheric Environment Solar Spectral Radiation (HESSR) model, to our SuperThermal Electron Transport (STET) model. In addition, we have proposed a new modification to the Hinteregger-81 model. The resultant photoelectron fluxes from the three solar irradiance models, the Hinteregger-81 model, FISM and the HESSR model, are compared and mostly vary within a factor of 2. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Xu, Shaosui; Liemohn, Michael W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Peterson, W. K.; Fontenla, Juan] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Chamberlin, Phillip] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Xu, SS (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM xussui@umich.edu
RI Peterson, WK/A-8706-2009; Chamberlin, Phillip/C-9531-2012;
OI Peterson, WK/0000-0002-1513-6096; Chamberlin,
Phillip/0000-0003-4372-7405; Xu, Shaosui/0000-0002-5121-600X
FU NASA; NSF [NNX13AG26G, AST-0908311]
FX The authors would like to thank NASA and NSF for their support of this
project under Grants NNX13AG26G and AST-0908311. The FISM solar
irradiance fluxes are available at http://lasp.colorado.edu/lisird/fism/
and the HESSR model data at
http://www.galactitech.net/hessrdata/Mars/Spectra/. The numerical data
and the current version of the SuperThermal Electron Transport (STET)
model are available upon request to the authors.
NR 36
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Z9 7
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC 15
PY 2015
VL 119
SI SI
BP 62
EP 68
DI 10.1016/j.pss.2015.09.008
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4YI
UT WOS:000367108700009
ER
PT J
AU Poppe, AR
Zimmerman, MI
Halekas, JS
Farrell, WM
AF Poppe, A. R.
Zimmerman, M. I.
Halekas, J. S.
Farrell, W. M.
TI The electrostatic plasma environment of a small airless body under
non-aligned plasma flow and UV conditions
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Surface charging/potentials; Airless bodies; Plasma interactions; Plasma
wakes; Photoelectron sheaths
ID SOLAR-WIND; PHOTOELECTRON SHEATH; SPACE; SIMULATION; FIELDS; WAKE;
SURFACE; DUST; MOON; RHEA
AB Airless bodies interact with a wide variety of plasma environments throughout the solar system. For many objects, incident plasma is nearly co-aligned with solar ultraviolet radiation leading to the development of a positively charged dayside photoelectron sheath and a negatively charged nightside plasma sheath. Other objects, however, are present in environments where the plasma flow and solar UV radiation may not co-align. These environments include, for example, the moons of Mars as they pass through the deflected Martian magnetosheath, and many of the moons of the outer planets, which are embedded in co-rotating planetary magnetospheres. The decoupling of the plasma flow and UV incidence vectors opens up a wide range of possible surface charging and near-object plasma conditions as a function of the relative plasma-UV incidence angle. Here, we report on a series of simulations of the plasma interaction of a small body (effectively smaller than both electron and ion gyroradii) with both flowing plasma and UV radiation for different plasma-UV incidence angles using an electrostatic treecode model. We describe the plasma and electric field environment both on the object surface and in the interaction region surrounding the object, including complex surface charge and electric field distributions, interactions between surface-generated photoelectrons and ambient plasma electrons, and complex potential distributions, all of which vary as a function of the relative plasma flow-UV angle. We also show that in certain conditions, non-monotonic potential structures may exist around such objects, partially similar to those found at Earth's Moon. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Poppe, A. R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Poppe, A. R.; Zimmerman, M. I.; Halekas, J. S.; Farrell, W. M.] NASA, Solar Syst Explorat Res Virtual Inst, Ames Res Ctr, Mountain View, CA USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
RI Farrell, William/I-4865-2013;
OI Halekas, Jasper/0000-0001-5258-6128
FU NASA's Solar System Exploration Research Virtual Institute (SSERVI)
[NNX14AG16A]
FX The authors gratefully acknowledge support from NASA's Solar System
Exploration Research Virtual Institute (SSERVI), grant #NNX14AG16A. This
publication is SSERVI contribution #SSERVI-2014-274. The authors also
acknowledge the International Space Science Institute (ISSI) for hosting
a workshop series that in part inspired this work. Finally, the authors
thank two reviewers for constructive comments.
NR 52
TC 0
Z9 0
U1 1
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC 15
PY 2015
VL 119
SI SI
BP 111
EP 120
DI 10.1016/j.pss.2015.06.001
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4YI
UT WOS:000367108700013
ER
PT J
AU Vandaele, AC
Neefs, E
Drummond, R
Thomas, IR
Daerden, F
Lopez-Moreno, JJ
Rodriguez, J
Patel, MR
Bellucci, G
Allen, M
Altieri, F
Bolsee, D
Clancy, T
Delanoye, S
Depiesse, C
Cloutis, AE
Fedorova, A
Formisano, V
Funke, B
Fussen, D
Geminale, A
Gerard, JC
Giuranna, M
Ignatiev, N
Kaminski, J
Karatekin, O
Lefevre, F
Lopez-Puertas, M
Lopez-Valverde, M
Mahieux, A
McConnell, J
Mumma, M
Neary, L
Renotte, E
Ristic, B
Robert, S
Smith, M
Trokhimovsky, S
Vander Auwera, J
Villanueva, G
Whiteway, J
Wilquet, V
Wolff, M
Vandaele, AC
Moreno, L
Juan, J
Bellucci, G
Patel, M
Allen, M
Altieri, F
Aoki, S
Bolsee, D
Clancy, T
Cloutis, E
Daerden, F
Depiesse, C
Fedorova, A
Formisano, V
Funke, B
Fussen, D
Garcia-Comas, M
Geminale, A
Gerard, JC
Gillotay, D
Giuranna, M
Gonzalez-Galindo, F
Ignatiev, N
Kaminski, J
Karatekin, O
Kasabe, Y
Lefevre, F
Lewis, S
Lopez-Puertas, M
Lopez-Valverde, M
Mahieux, A
Mason, J
Mumma, M
Neary, L
Neefs, E
Smith, M
Thomas, IR
Trokhimovsky, S
Vander Auwera, J
Villanueva, G
Whiteway, J
Willame, Y
Wilquet, V
Wolff, M
Alonso-Rodrigo, G
Moral Beatriz, D
Barzin, P
BenMoussa, A
Berkenbosch, S
Biondi, D
Bonnewijn, S
Candini, GP
Clairquin, R
Cubas, J
Delanoye, S
Giordanengo, B
Gissot, S
Gomez, A
Zafra, JJ
Leese, M
Maes, J
Mazy, E
Mazzoli, A
Meseguer, J
Orban, A
Pastor-Morales, MD
Perez-Grande, I
Ristic, B
Rodriguez-Gomez, J
Saggin, B
Samain, V
Sanz Andres, A
Sanz, R
Simar, JF
Thibert, T
AF Vandaele, A. C.
Neefs, E.
Drummond, R.
Thomas, I. R.
Daerden, F.
Lopez-Moreno, J. -J.
Rodriguez, J.
Patel, M. R.
Bellucci, G.
Allen, M.
Altieri, F.
Bolsee, D.
Clancy, T.
Delanoye, S.
Depiesse, C.
Cloutis, A. E.
Fedorova, A.
Formisano, V.
Funke, B.
Fussen, D.
Geminale, A.
Gerard, J. -C.
Giuranna, M.
Ignatiev, N.
Kaminski, J.
Karatekin, O.
Lefevre, F.
Lopez-Puertas, M.
Lopez-Valverde, M.
Mahieux, A.
McConnell, J.
Mumma, M.
Neary, L.
Renotte, E.
Ristic, B.
Robert, S.
Smith, M.
Trokhimovsky, S.
Vander Auwera, J.
Villanueva, G.
Whiteway, J.
Wilquet, V.
Wolff, M.
Vandaele, Ann Carine
Moreno, Lopez
Juan, Jose
Bellucci, Giancarlo
Patel, Manish
Allen, Mark
Altieri, Francesca
Aoki, Shohei
Bolsee, David
Clancy, Todd
Cloutis, Edward
Daerden, Frank
Depiesse, Cedric
Fedorova, Anna
Formisano, Vittorio
Funke, Bernd
Fussen, Didier
Garcia-Comas, Maya
Geminale, Anna
Gerard, Jean-Claude
Gillotay, Didier
Giuranna, Marco
Gonzalez-Galindo, Francisco
Ignatiev, Nicolai
Kaminski, Jacek
Karatekin, Ozgur
Kasabe, Yasumasa
Lefevre, Franck
Lewis, Stephen
Lopez-Puertas, Manuel
Lopez-Valverde, Miguel
Mahieux, Arnaud
Mason, Jon
Mumma, Mike
Neary, Lori
Neefs, Eddy
Smith, Mike
Thomas, Ian R.
Trokhimovsky, Sacha
Vander Auwera, Jean
Villanueva, Geronimo
Whiteway, Jim
Willame, Yannick
Wilquet, Valerie
Wolff, Mike
Alonso-Rodrigo, Gustavo
Aparicio del Moral, Beatriz
Barzin, Pascal
BenMoussa, Ali
Berkenbosch, Sophie
Biondi, David
Bonnewijn, Sabrina
Candini, Gian Paolo
Clairquin, Roland
Cubas, Javier
Delanoye, Sofie
Giordanengo, Boris
Gissot, Samuel
Gomez, Alejandro
Zafra, Jose-Jeronimo
Leese, Mark
Maes, Jeroen
Mazy, Emmanuel
Mazzoli, Alexandra
Meseguer, Jose
Orban, Anne
Pastor-Morales, Maria del Carmen
Perez-Grande, Isabel
Ristic, Bojan
Rodriguez-Gomez, Julio
Saggin, Bortolino
Samain, Valerie
Sanz Andres, Angel
Sanz, Rosario
Simar, Juan-Felipe
Thibert, Tanguy
CA NOMAD Team
TI Science objectives and performances of NOMAD, a spectrometer suite for
the ExoMars TGO mission
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE ExoMars; Solar occultation; Nadir observations; Mars atmosphere;
Composition; Infrared; Ultraviolet; Visible; Spectroscopy; Methane;
Aerosol
ID 3.3 MU-M; MARTIAN ATMOSPHERE; WATER-VAPOR; VENUS-EXPRESS; SENSITIVE
SEARCH; SOLAR OCCULTATION; TUNABLE FILTER; OPTICAL DEPTH; ISOTOPIC CO2;
UPPER LIMITS
AB The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition and distribution of Mars' atmospheric trace species in unprecedented detail, fulfilling many of the scientific objectives of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument is a combination of three channels, covering a spectral range from the UV to the IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and how these objectives have influenced the design of the channels. We also discuss the expected performance of the instrument in terms of coverage and detection sensitivity. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Vandaele, A. C.; Neefs, E.; Drummond, R.; Thomas, I. R.; Daerden, F.; Bolsee, D.; Delanoye, S.; Depiesse, C.; Fussen, D.; Mahieux, A.; Neary, L.; Ristic, B.; Robert, S.; Wilquet, V.; Vandaele, Ann Carine] Belgian Inst Space Aeron IASB BIRA, Ave Circulaire 3, B-1180 Brussels, Belgium.
[Lopez-Moreno, J. -J.; Rodriguez, J.; Funke, B.; Lopez-Puertas, M.; Lopez-Valverde, M.; Juan, Jose] Inst Astrofis Andalucia IAA CSIC, Granada, Spain.
[Patel, M. R.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Bellucci, G.; Altieri, F.; Formisano, V.; Geminale, A.; Giuranna, M.] Ist Astrofis & Planetol Spaziali IAPS INAF, I-00133 Rome, Italy.
[Allen, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Clancy, T.; Wolff, M.] Space Sci Inst, Boulder, CO 80301 USA.
[Cloutis, A. E.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Fedorova, A.; Ignatiev, N.; Trokhimovsky, S.] IKI, Moscow, Russia.
[Gerard, J. -C.] Univ Liege, Liege, Belgium.
[Kaminski, J.; McConnell, J.; Whiteway, J.] York Univ, N York, ON M3J 1P3, Canada.
[Karatekin, O.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Lefevre, F.] CNR5, LATMOS, Paris, France.
[Mumma, M.; Smith, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Renotte, E.] Ctr Spatial Liege, Liege, Belgium.
[Vander Auwera, J.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, Brussels, Belgium.
[Villanueva, G.] Catholic Univ Amer, Washington, DC 20064 USA.
[Patel, M. R.] STFC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
RP Vandaele, AC (reprint author), Belgian Inst Space Aeron IASB BIRA, Ave Circulaire 3, B-1180 Brussels, Belgium.
EM a-c.vandaele@aeronomie.be
RI Funke, Bernd/C-2162-2008; Perez Grande, Isabel/L-2243-2014;
Gonzalez-Galindo, Francisco/I-2495-2015;
OI Funke, Bernd/0000-0003-0462-4702; Perez Grande,
Isabel/0000-0002-7145-2835; Gonzalez-Galindo,
Francisco/0000-0001-9443-291X; Aparicio del Moral,
Beatriz/0000-0003-2817-8719; Lopez-Valverde, M. A./0000-0002-7989-4267;
saggin, bortolino/0000-0002-4033-3585; Lewis,
Stephen/0000-0001-7237-6494; GERARD, Jean-Claude/0000-0002-8565-8746
FU Belgian Science Policy Office (BELSPO); ESA Prodex Office [PEA
4000107727]; Belgian government; Plan Nacional [AYA2012-39691-C02-01,
AYA2012-39691-C02-02]; UK Space Agency [ST/I003061/1]
FX NOMAD has been made possible thanks to funding by the Belgian Science
Policy Office (BELSPO) and financial and contractual coordination by the
ESA Prodex Office (Grant number: PEA 4000107727). The research was
performed as part of the "Interuniversity Attraction Poles" program
financed by the Belgian government (Planet TOPERS). Spanish
Institutions, IAA-CSIC and IDR-UPM were funded by Plan Nacional under
Projects AYA2012-39691-C02-01 and 02. UK funding is acknowledged under
the UK Space Agency grant ST/I003061/1.
NR 117
TC 5
Z9 5
U1 1
U2 20
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC 15
PY 2015
VL 119
SI SI
BP 233
EP 249
DI 10.1016/j.pss.2015.10.003
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4YI
UT WOS:000367108700024
ER
PT J
AU de Moura, YM
Hilker, T
Lyapustin, AI
Galva, LS
dos Santos, JR
Anderson, LO
de Sousa, CHR
Arai, E
AF de Moura, Yhasmin Mendes
Hilker, Thomas
Lyapustin, Alexei I.
Galva, Lenio Soares
dos Santos, Joao Roberto
Anderson, Liana O.
Resende de Sousa, Celio Helder
Arai, Egidio
TI Seasonality and drought effects of Amazonian forests observed from
multi-angle satellite data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Amazon; Drought; Anisotropy; Greening; Browning; MAIAC; MODIS
ID LEAF-AREA INDEX; RADIATIVE-TRANSFER PROBLEM; NON-LAMBERTIAN SURFACE;
DRY-SEASON; CANOPY STRUCTURE; ATMOSPHERIC CORRECTION; RAIN-FORESTS;
BIDIRECTIONAL REFLECTANCE; VEGETATION STRUCTURE; TROPICAL FOREST
AB Seasonality and drought in Amazon rainforests have been controversially discussed in the literature, partially due to a limited ability of current remote sensing techniques to detect its impacts on tropical vegetation. We use a multi-angle remote sensing approach to determine changes in vegetation structure from differences in directional scattering (anisotropy) observed by the Moderate Resolution Imaging Spectroradiometer (MODIS) with data atmospherically corrected by the Multi-Angle Implementation Atmospheric Correction Algorithm (MAIAC). Our results show a strong linear relationship between anisotropy and field (r(2) = 0.70) and LiDAR (r(2) = 0.88) based estimates of LAI even in dense canopies (LAI <= 7 m(2) m(-2)). This allowed us to obtain improved estimates of vegetation structure from optical remote sensing. We used anisotropy to analyze Amazon seasonality based on spatially explicit estimates of onset and length of dry season obtained from the Tropical Rainfall Measurement Mission (TRMM). An increase in vegetation greening was observed during the beginning of dry season (across similar to 7% of the basin), which was followed by a decline (browning) later during the dry season (across similar to 5% of the basin). Anomalies in vegetation browning were particularly strong during the 2005 and 2010 drought years (similar to 10% of the basin). We show that the magnitude of seasonal changes can be significantly affected by regional differences in onset and duration of the dry season. Seasonal changes were much less pronounced when assuming a fixed dry season from June through September across the Amazon Basin. Our findings reconcile remote sensing studies with field based observations and model results as they provide a sounder basis for the argument that tropical vegetation growth increases during the beginning of the dry season, but declines after extended drought periods. The multi-angle approach used in this work may help quantify drought tolerance and seasonality in the Amazonian forests. (C) 2015 Elsevier Inc. All rights reserved.
C1 [de Moura, Yhasmin Mendes; Galva, Lenio Soares; dos Santos, Joao Roberto; Arai, Egidio] Natl Inst Space Res INPE, Sao Jose Dos Campos, SP, Brazil.
[Hilker, Thomas; Resende de Sousa, Celio Helder] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Liana O.] Natl Ctr Monitoring & Early Warning Nat Disasters, Sao Jose Dos Campos, SP, Brazil.
[Anderson, Liana O.] Univ Oxford, Environm Change Inst, Oxford OX1 3QY, England.
RP de Moura, YM (reprint author), Natl Inst Space Res INPE, Ave Astronautas 1758, Sao Jose Dos Campos, SP, Brazil.
EM yhas.mendes@gmail.com
OI Moura, Yhasmin/0000-0001-8494-8787; Anderson, Liana/0000-0001-9545-5136
FU CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior)
[12881-13-9]; CNPq (Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico) [PVE 401025/2014-4]; UK NERC Amazonica [NE/F005482/1];
FAPESP [2013/50533-5]
FX We are grateful to the NASA Center for Climate Simulation (NCCS) for
computational support and access to their high performance cluster.
MAIAC data for the Amazon Basin was obtained from NASA's Level 1
Atmosphere Archive and Distribution System (LAADS Web) ftp://ladsweb.
nascom.nasa.gov/MAIAC. We would like to thank Dr. Michael Keller for the
helpful comments. LiDAR data for this study were obtained from the
"Sustainable Landscapes Brazil" project, operated as a cooperation
between EMBRAPA and the U.S. Forest Service
(http://mapas.cnpm.embrapa.br/paisagenssustentaveis/). This study was
partially funded by CAPES (Coordenacao de Aperfeicoamento de Pessoal de
Nivel Superior), grant number 12881-13-9; and CNPq (Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico), grant number PVE
401025/2014-4. L.O.A thanks UK NERC Amazonica grant NE/F005482/1 and
FAPESP grant 2013/50533-5.
NR 91
TC 1
Z9 1
U1 6
U2 33
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 15
PY 2015
VL 171
BP 278
EP 290
DI 10.1016/j.rse.2015.10.015
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ0IE
UT WOS:000366787600022
ER
PT J
AU Wedemeyer, S
Bastian, T
Brajsa, R
Barta, M
Hudson, H
Fleishman, G
Loukitcheva, M
Fleck, B
Kontar, E
De Pontieu, B
Tiwari, S
Kato, Y
Soler, R
Yagoubov, P
Black, JH
Antolin, P
Gunar, S
Labrosse, N
Benz, AO
Nindos, A
Steffen, M
Scullion, E
Doyle, JG
Zaqarashvili, T
Hanslmeier, A
Nakariakov, VM
Heinzel, P
Ayres, T
Karlicky, M
AF Wedemeyer, S.
Bastian, T.
Brajsa, R.
Barta, M.
Hudson, H.
Fleishman, G.
Loukitcheva, M.
Fleck, B.
Kontar, E.
De Pontieu, B.
Tiwari, S.
Kato, Y.
Soler, R.
Yagoubov, P.
Black, J. H.
Antolin, P.
Gunar, S.
Labrosse, N.
Benz, A. O.
Nindos, A.
Steffen, M.
Scullion, E.
Doyle, J. G.
Zaqarashvili, T.
Hanslmeier, A.
Nakariakov, V. M.
Heinzel, P.
Ayres, T.
Karlicky, M.
CA SSALMON Grp
TI SSALMON - The Solar Simulations for the Atacama Large Millimeter
Observatory Network
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Solar atmosphere; Chromosphere; Millimeter radiation; ALMA
ID CARBON-MONOXIDE; ALFVEN WAVES; QUIET-SUN; INTERFEROMETER OBSERVATIONS;
TRANSVERSE OSCILLATIONS; QUIESCENT PROMINENCE; RESONANT ABSORPTION;
MAGNETIC-STRUCTURE; CORONAL LOOPS; COOL STARS
AB The Solar Simulations for the Atacama Large Millimeter Observatory Network (SSALMON) was initiated in 2014 in connection with two ALMA development studies. The Atacama Large Millimeter/submillimeter Array (ALMA) is a powerful new tool, which can also observe the Sun at high spatial, temporal, and spectral resolution. The international SSALMONetwork aims at co-ordinating the further development of solar observing modes for ALMA and at promoting scientific opportunities for solar physics with particular focus on numerical simulations, which can provide important constraints for the observing modes and can aid the interpretation of future observations. The radiation detected by ALMA originates mostly in the solar chromosphere a complex and dynamic layer between the photosphere and corona, which plays an important role in the transport of energy and matter and the heating of the outer layers of the solar atmosphere. Potential targets include active regions, prominences, quiet Sun regions, flares. Here, we give a brief overview over the network and potential science cases for future solar observations with ALMA. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Wedemeyer, S.; Kato, Y.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Wedemeyer, S.; Brajsa, R.; Barta, M.; Karlicky, M.] Astron Inst ASCR, European ARC, Czech Node, Ondrejov, Czech Republic.
[Bastian, T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Brajsa, R.] Univ Zagreb, Fac Geodesy, Hvar Observ, Zagreb 10000, Croatia.
[Barta, M.; Gunar, S.; Heinzel, P.; Karlicky, M.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic.
[Hudson, H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Hudson, H.; Kontar, E.; Labrosse, N.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Fleishman, G.] New Jersey Inst Technol, Dept Phys, Ctr Solar Terr Res, Newark, NJ 07102 USA.
[Loukitcheva, M.] St Petersburg Univ, Astron Inst, St Petersburg 198504, Russia.
[Loukitcheva, M.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Fleck, B.] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
[De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Tiwari, S.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Soler, R.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
[Yagoubov, P.] European Org Astron Res Southern Hemisphere ESO, D-85748 Garching, Germany.
[Black, J. H.] Chalmers, Dept Earth & Space Sci, Gothenburg, Sweden.
[Antolin, P.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Gunar, S.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[Benz, A. O.] Inst 4D Technol, FHNW, CH-5210 Windisch, Switzerland.
[Nindos, A.] Univ Ioannina, Dept Phys, GR-45110 Ioannina, Greece.
[Steffen, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Scullion, E.] Univ Dublin Trinity Coll, Dublin 2, Ireland.
[Doyle, J. G.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Zaqarashvili, T.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Hanslmeier, A.] Graz Univ, Inst Phys, A-8010 Graz, Austria.
[Nakariakov, V. M.] Univ Warwick, Dept Phys, Ctr Fus Space & Astrophys, Coventry CV4 7AL, W Midlands, England.
[Ayres, T.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
RP Wedemeyer, S (reprint author), Univ Oslo, Inst Theoret Astrophys, Postboks 1029 Blindern, N-0315 Oslo, Norway.
EM svenwe@astro.uio.no
RI Kontar, Eduard/B-7897-2008; Nakariakov, Valery/E-2375-2013; Labrosse,
Nicolas/B-2670-2010; Loukitcheva, Maria/I-6110-2013;
OI Kontar, Eduard/0000-0002-8078-0902; Nakariakov,
Valery/0000-0001-6423-8286; Labrosse, Nicolas/0000-0002-4638-157X;
Loukitcheva, Maria/0000-0001-5246-9044; Hudson, Hugh/0000-0001-5685-1283
FU Faculty of Mathematics and Natural Sciences of the University of Oslo,
Norway; Research Council of Norway [221767/F20]; European Commission
through the CIG Grant [PCIG-GA-2011-304265]; European Commission through
the GACR Grant [13-24782S]; European Commission eHEROES [284461];
European Commission SOLARNET [312495]; Croatian Science Foundation
[6212]; Marie Curie Radio Sun project [PIRSES-GA-2011-295272]; NSF
[AGS-1250374, AGS-1262772]; NASA [NNX14AC87G]; Saint Petersburg State
University [6.0.26.2010, 6.37.343.2015]; RFBR [15-02-03835]; European
Union (European Social Fund-ESF); Greek national funds through the
Operational Program "Education and Lifelong Learning" of the National
Strategic Reference Framework (NSRF) Research Funding Program: "Thales
FX S. Wedemeyer acknowledges support (UiO-PES2020) by the Faculty of
Mathematics and Natural Sciences of the University of Oslo, Norway, and
the Research Council of Norway (Grant 221767/F20).M. Barta thanks for
the support of the European Commission through the CIG Grant
PCIG-GA-2011-304265 (SERAF) and GACR Grant 13-24782S.Roman Brajsa
acknowledges support from the European Commission FP7 projects eHEROES
(284461, 2012-2015) and SOLARNET (312495, 2013-2017), as well as from
the Croatian Science Foundation (project 6212 "Solar and Stellar
Variability").M. Barta, M. Karlicky, E. Kontar and V. M. Nakariakov
acknowledge the Marie Curie PIRSES-GA-2011-295272 Radio Sun project.G.
Fleishman is supported by NSF Grants AGS-1250374 and AGS-1262772 and
NASA Grant NNX14AC87G to the New Jersey Institute of Technology.M.
Loukitcheva acknowledges Saint Petersburg State University for research
Grants 6.0.26.2010 and 6.37.343.2015, and Grant RFBR 15-02-03835.A
Nindos' work has been partly co-financed by the European Union (European
Social Fund-ESF) andGreek national funds through the Operational Program
"Education and Lifelong Learning" of the National Strategic Reference
Framework (NSRF) Research Funding Program: "Thales. Investing in
knowledge society through the European Social Fund".
NR 119
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U2 7
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 DEC 15
PY 2015
VL 56
IS 12
BP 2679
EP 2692
DI 10.1016/j.asr.2015.05.027
PG 14
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CZ0AT
UT WOS:000366768200002
ER
PT J
AU Pevtsov, AA
Bertello, L
MacNeice, P
AF Pevtsov, Alexei A.
Bertello, Luca
MacNeice, Peter
TI Effect of uncertainties in solar synoptic magnetic flux maps in modeling
of solar wind
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Solar magnetic fields; Uncertainties; Solar wind; Modeling
AB Recently, the NSO/SOLIS team developed variance (error) maps that represent uncertainties in magnetic flux synoptic charts. These uncertainties are determined by the spatial variances of the magnetic flux distribution from full disk magnetograms that contribute to each bin in the synoptic chart. Here we present a study of the effects of variances on solar wind parameters (wind speed, density, magnetic field, and temperature) derived using the WSA-ENLIL model and ensemble modeling approach. We compare the results of the modeling with near-Earth solar wind magnetic field and plasma data as extracted from NASA/GSFC's OMNI data set. We show that analysis of uncertainties may be useful for understanding the sensitivity of the model predictions to short-term evolution of magnetic field and noise in the synoptic magnetograms. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Pevtsov, Alexei A.] Natl Solar Observ, Sunspot, NM 88349 USA.
[Bertello, Luca] Natl Solar Observ, Tucson, AZ 85719 USA.
[MacNeice, Peter] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Pevtsov, AA (reprint author), Natl Solar Observ, 3010 Coronal Loop, Sunspot, NM 88349 USA.
EM apevtsov@nso.edu; lbertello@nso.edu; Peter.J.Macneice@nasa.gov
OI Pevtsov, Alexei/0000-0003-0489-0920
FU NASA [NNH14AX891]
FX The National Solar Observatory (NSO) is operated by the Association of
Universities for Research in Astronomy, AURA Inc under cooperative
agreement with the National Science Foundation (NSF). Data were acquired
by VSM/SOLIS operated by NISP/NSO/AURA/NSF. Development of synoptic
charts of uncertainties was partially supported by NASA NNH14AX891
award. The authors acknowledge constructive comments by the anonymous
reviewers that led to an improvement of this article.
NR 14
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U1 0
U2 1
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 DEC 15
PY 2015
VL 56
IS 12
BP 2719
EP 2726
DI 10.1016/j.asr.2015.05.043
PG 8
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CZ0AT
UT WOS:000366768200006
ER
PT J
AU Greenberger, RN
Mustard, JF
Cloutis, EA
Mann, P
Wilson, JH
Flemming, RL
Robertson, KM
Salvatore, MR
Edwards, CS
AF Greenberger, Rebecca N.
Mustard, John F.
Cloutis, Edward A.
Mann, Paul
Wilson, Janette H.
Flemming, Roberta L.
Robertson, Kevin M.
Salvatore, Mark R.
Edwards, Christopher S.
TI Hydrothermal alteration and diagenesis of terrestrial lacustrine pillow
basalts: Coordination of hyperspectral imaging with laboratory
measurements
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ROCK-FORMING MINERALS; NEAR-INFRARED SPECTRA; HARTFORD RIFT BASIN;
REFLECTANCE SPECTROSCOPY; CARBONATE MINERALS; RAMAN-SPECTROSCOPY;
NORTHEASTERN USA; MESOZOIC BASALTS; MIDOCEAN RIDGES; OCEANIC-CRUST
AB We investigate an outcrop of similar to 187 Ma lacustrine pillow basalts of the Talcott Formation exposed in Meriden, Connecticut, USA, focusing on coordinated analyses of one pillow lava to characterize the aqueous history of these basalts in the Hartford Basin. This work uses a suite of multidisciplinary measurements, including hyperspectral imaging, other spectroscopic techniques, and chemical and mineralogical analyses, from the microscopic scale up to the scale of an outcrop.
The phases identified in the sample are albite, large iron oxides, and titanite throughout; calcite in vesicles; calcic clinopyroxene, aegirine, and Fe/Mg-bearing clay in the rind; and fine-grained hematite and pyroxenes in the interior. Using imaging spectroscopy, the chemistry and mineralogy results extend to the hand sample and larger outcrop. From all of the analyses, we suggest that the pillow basalts were altered initially after emplacement, either by heated lake water or magmatic fluids, at temperatures of at least 400-600 degrees C, and the calcic clinopyroxenes and aegirine identified in the rind are a preserved record of that alteration. As the hydrothermal system cooled to slightly lower temperatures, clays formed in the rind, and, during this alteration, the sample oxidized to form hematite in the matrix of the interior and Fe3+ in the pyroxenes in the rind. During the waning stages of the hydrothermal system, calcite precipitated in vesicles within the rind. Later, diagenetic processes albitized the sample, with albite replacing plagioclase, lining vesicles, and accreting onto the exterior of the sample. This albitization or Na-metasomatism occurred when the lake within the Hartford Basin evaporated during a drier past climatic era, resulting in Na-rich brines. As Ca-rich plagioclase altered to albite, Ca was released into solution, eventually precipitating as calcite in previously-unfilled vesicles, dominantly in the interior of the pillow. Coordinated analyses of this sample permit identification of the alteration phases and help synthesize the aqueous history of pillow lavas of the Talcott Formation. These results are also relevant to Mars, where volcanically-resurfaced open basin lakes have been found, and this Hartford Basin outcrop may be a valuable analog for any potential volcano-lacustrine interactions. The results can also help to inform the utility and optimization of potentially complementary, synergistic, and uniquely-suited techniques for characterization of hydrothermally-altered terrains. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Greenberger, Rebecca N.; Mustard, John F.; Robertson, Kevin M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Cloutis, Edward A.; Mann, Paul] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Wilson, Janette H.] Headwall Photon Inc, Fitchburg, MA 01420 USA.
[Flemming, Roberta L.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada.
[Salvatore, Mark R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Edwards, Christopher S.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
RP Greenberger, RN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 306-431, Pasadena, CA 91109 USA.
EM Rebecca.N.Greenberger@jpl.nasa.gov
OI Greenberger, Rebecca/0000-0003-1583-0261
FU NASA; Mars Data Analysis Program [NNX13AK72G]; NSERC; University of
Winnipeg
FX We would like to thank Anthony Philpotts for showing us potential field
sites and Kevin Cannon, Tim Goudge, Mary Peterson, and Sandra Wiseman
for field assistance. We also thank David Bannon and Kwok Wong at
Headwall Photonics, Inc. for assistance with laboratory hyperspectral
imaging measurements; Joe Boesenberg, Bill Collins, and Terik Daly for
help with thin and thick section preparation and electron microprobe
analyses; Dave Murray and Joe Orchardo for help with bulk chemical
analyses; Gordon Osinski for suggesting lXRD analyses and Alex
Pontefract for arranging and assisting with them; Phil Christensen for
his effort in building Arizona State University's MicroSpectroscopy Lab
in which the microscopic thermal emission measurements were made and
Rebecca Smith for help with those measurements; and Reid Cooper for
helpful discussions. Finally, we thank Target in Meriden, Connecticut,
for allowing us to work on their property and the City of Meriden for
permitting sampling. We are grateful for the critical and constructive
comments by two anonymous reviewers, Associate Editor Wolf Uwe Reimold,
and Executive Editor Marc Norman. This work was supported by NASA and
the Mars Data Analysis Program grant NNX13AK72G. E.A.C. thanks CFI,
MRIF, and CSA for supporting the establishment of the University of
Winnipeg Planetary Spectrophotometer Facility, as well as these agencies
and NSERC and University of Winnipeg for funding to support this study.
Any use of trade, firm, or product names is for descriptive purposes
only and does not imply endorsement by the U.S. Government.
NR 123
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD DEC 15
PY 2015
VL 171
BP 174
EP 200
DI 10.1016/j.gca.2015.08.024
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CW2KW
UT WOS:000364822100011
ER
PT J
AU Hanna, RD
Ketcham, RA
Zolensky, M
Behr, WM
AF Hanna, Romy D.
Ketcham, Richard A.
Zolensky, Mike
Behr, Whitney M.
TI Impact-induced brittle deformation, porosity loss, and aqueous
alteration in the Murchison CM chondrite
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ELECTRON BACKSCATTER DIFFRACTION; CV CARBONACEOUS CHONDRITES; RAY
COMPUTED-TOMOGRAPHY; PREFERRED ORIENTATION; SHOCK METAMORPHISM;
DIFFERENTIATED PLANETESIMALS; MAGNETIC-ANISOTROPY; PARENT BODIES; SOLAR
NEBULA; CHONDRULES
AB X-ray computed tomographic scanning of a 44 g Murchison stone (USNM 5487) reveals a preferred alignment of deformed, partially altered chondrules, which define a prominent foliation and weak lineation in 3D. The presence of a lineation and evidence for a component of rotational, noncoaxial shear suggest that the deformation was caused by impact. Olivine optical extinction indicates that the sample can be classified as shock stage S1, and electron backscatter diffraction (EBSD) and electron microscopy reveal that plastic deformation within the chondrules was minimal and that brittle deformation in the form of fracturing, cataclasis, and grain boundary sliding was the dominant microstructural strain-accommodating mechanism. Textural evidence such as serpentine veins parallel to the foliation fabric and crosscutting alteration veins strongly suggest that some aqueous alteration post-dated or was contemporaneous with the deformation and that multiple episodes of fracturing and mineralization occurred. Finally, using the deformed shape of the chondrules we estimate that the strain experienced by Murchison was 17-43%. This combined with the current measured porosity of Murchison suggests that the original bulk porosity of Murchison prior to its deformation was 32.2-53.4% and likely at the upper end of this range due to chondrule compressibility, providing a unique estimate of pre-deformation porosity for a carbonaceous chondrite. Our findings suggest that significant porosity loss, deformation, and compaction from impact can occur on chondrite parent bodies whose samples may record only a low level of shock, and that significant chondrule deformation resulting in a chondrite foliation fabric can occur primarily through brittle processes and does not require plastic deformation of grains. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Hanna, Romy D.; Ketcham, Richard A.; Behr, Whitney M.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA.
[Zolensky, Mike] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA.
RP Hanna, RD (reprint author), Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA.
EM romy@jsg.utexas.edu
RI Ketcham, Richard/B-5431-2011;
OI Ketcham, Richard/0000-0002-2748-0409; behr, Whitney/0000-0002-3003-8670
FU NASA [NNX13AO64H]; Jackson School of Geosciences
FX We would like to express our sincere gratitude to the Smithsonian
National Museum of Natural History, curator Tim McCoy, and collection
manager Linda Welzenbach for the loan of Murchison USNM 5487 and for
authorizing and providing new section cuts for this project. We would
like to thank Associate Editor Eric Quirico, Alan Rubin, and an
anonymous reviewer for thoughtful comments that greatly improved this
manuscript. Thanks to James Martinez (JSC) for assistance with EBSD and
section polishing, to Travis Clow and Zoe Yin (Univ. Texas at Austin)
for assistance in Avizo (TM) segmentation and testing, and to John Hanna
for help with the generation of Fig. 16. Thanks to Paula Lindgren, Jon
Friedrich, Martin Lee, Alex Ruzicka and Lindy Elkins-Tanton for helpful
discussions regarding a variety of topics related to the paper. R.D.H.
is supported by the NASA Earth and Space Sciences Fellowship Program -
Grant NNX13AO64H and portions of this work were funded through an
Analytical Fees grant from the Jackson School of Geosciences to R.D.H.,
M.E.Z. was supported by a grant from the NASA Cosmochemistry Program.
NR 91
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U1 3
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD DEC 15
PY 2015
VL 171
BP 256
EP 282
DI 10.1016/j.gca.2015.09.005
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CW2KW
UT WOS:000364822100015
ER
PT J
AU Emory, AE
McLinden, M
Schreier, M
Wick, GA
AF Emory, Amber E.
McLinden, Matthew
Schreier, Mathias
Wick, Gary A.
TI AN INTRODUCTION TO THE NASA EAST PACIFIC ORIGINS AND CHARACTERISTICS OF
HURRICANES (EPOCH) FIELD CAMPAIGN
SO TROPICAL CYCLONE RESEARCH AND REVIEW
LA English
DT Article
ID RAPID INTENSIFICATION; AIRCRAFT; SYSTEM; CORE
AB Over the past five years, tropical activity in the East Pacific has increased, while declining in the Atlantic Basin. In addition, during El Nino years, warmer than average sea surface temperatures further increase the likelihood of tropical cyclone formation in the East Pacific. Hurricane field campaigns used the Ku-/Ka-band HighAltitude Wind and Rain Airborne Profiler (HIWRAP) radar on the Global Hawk (GH) unmanned aircraft, in GRIP (Genesis and Rapid Intensification Processes 2010), HS3 (Hurricane and Severe Storm Sentinel 2012-14), and the NOAA Sensing Hazards with Operational Unmanned Technology (SHOUT 2015-16) field campaigns. Although originally designed for the GH, the X-band high-altitude RADar (EXRAD) has yet to be integrated and flown on an unmanned aerial vehicle. EXRAD will provide data with less attenuation of signal over deep convection as well as better estimates of three-dimensional winds with its nadir-pointing beam. As part of the NASA Hand On Project Experience (HOPE) Training Opportunity, our team proposed to fly the AV-6 GH aircraft with the EXRAD radar, the High Altitude MMIC Sounding Radiometer (HAMSR), and NOAA Advanced Vertical Atmospheric Profiling System (AVAPS) dropsondes to investigate genesis and/or rapid intensification (RI) of an East Pacific hurricane by measuring both the environment and interior structures. Information on planned activities primarily focused on the EXRAD high-altitude radar integration for the July-August 2017 science flight will be presented.
C1 [Emory, Amber E.; McLinden, Matthew] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Schreier, Mathias] Jet Prop Lab, Pasadena, CA USA.
[Wick, Gary A.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Emory, AE (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM amber.emory@nasa.gov
NR 34
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U1 0
U2 0
PU ESCAP-WMO TYPHOON COMMITTEE
PI MACAU
PA ESCAP-WMO TYPHOON COMMITTEE, MACAU, 00000, PEOPLES R CHINA
SN 2225-6032
J9 TROP CYCLONE RES REV
JI Trop. Cyclone Res. Rev.
PD DEC 15
PY 2015
VL 4
IS 3-4
BP 124
EP 131
DI 10.6057/2015TCRRh3.03
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL7ZW
UT WOS:000394840900003
ER
PT J
AU Verma, M
Friedl, MA
Law, BE
Bonal, D
Kiely, G
Black, TA
Wohlfahrt, G
Moors, EJ
Montagnani, L
Marcolla, B
Toscano, P
Varlagin, A
Roupsard, O
Cescatti, A
Arain, MA
D'Odorico, P
AF Verma, M.
Friedl, M. A.
Law, B. E.
Bonal, D.
Kiely, G.
Black, T. A.
Wohlfahrt, G.
Moors, E. J.
Montagnani, L.
Marcolla, B.
Toscano, P.
Varlagin, A.
Roupsard, O.
Cescatti, A.
Arain, M. A.
D'Odorico, P.
TI Improving the performance of remote sensing models for capturing intra-
and inter-annual variations in daily GPP: An analysis using global
FLUXNET tower data
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Gross primary productivity; Remote sensing; Modeling; FLUXNET; Seasonal;
Lagged effects
ID GROSS PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; EDDY COVARIANCE DATA;
IMAGING SPECTRORADIOMETER DATA; ENHANCED VEGETATION INDEX; LAND-SURFACE
TEMPERATURE; NET ECOSYSTEM EXCHANGE; PRIMARY PRODUCTIVITY;
CARBON-DIOXIDE; TERRESTRIAL GROSS
AB Accurate and reliable estimates of gross primary productivity (GPP) are required for monitoring the global carbon cycle at different spatial and temporal scales. Because GPP displays high spatial and temporal variation, remote sensing plays a major role in producing gridded estimates of GPP across spatiotemporal scales. In this context, understanding the strengths and weaknesses of remote sensing-based models of GPP and improving their performance is a key contemporary scientific activity. We used measurements from 157 research sites (similar to 470 site-years) in the FLUXNET "La Thuile" data and compared the skills of 11 different remote sensing models in capturing intra- and inter-annual variations in daily GPP in seven different biomes. Results show that the models were able to capture significant intra-annual variation in GPP (Index of Agreement = 0.4-0.80) in all biomes. However, the models' ability to track inter-annual variation in daily GPP was significantly weaker (IoA < 0.45). We examined whether the inclusion of different mechanisms that are missing in the models could improve their predictive power. The mechanisms included the effect of sub-daily variation in environmental variables on daily GPP, factoring-in differential rates of GPP conversion efficiency for direct and diffuse incident radiation, lagged effects of environmental variables, better representation of soil-moisture dynamics, and allowing spatial variation in model parameters. Our analyses suggest that the next generation remote sensing models need better representation of soil-moisture, but other mechanisms that have been found to influence GPP in site-level studies may not have significant bearing on model performance at continental and global scales. Understanding the relative controls of biotic vis-a-vis abiotic factors on GPP and accurately scaling up leaf level processes to the ecosystem scale are likely to be important for recognizing the limitations of remote sensing model and improving their formulation. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Verma, M.; Friedl, M. A.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Verma, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Law, B. E.] Oregon State Univ, Earth Syst Sci Div, Corvallis, OR 97331 USA.
[Bonal, D.] UMR EEF Univ Lorraine INRA, INRA Nancy, F-54280 Champenoux, France.
[Kiely, G.] Natl Univ Ireland Univ Coll Cork, Environm Res Inst, Civil & Environm Engn Dept, Cork, Ireland.
[Black, T. A.] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada.
[Wohlfahrt, G.] Univ Innsbruck, Inst Ecol, A-6020 Innsbruck, Austria.
[Wohlfahrt, G.] European Acad Bolzano, I-39100 Bolzano, Italy.
[Moors, E. J.] Alterra Wageningen UR, Climate Change & Adapt Land & Water Management, NL-6700 AA Wageningen, Netherlands.
[Montagnani, L.] Free Univ Bolzano Bozen, Fac Sci & Technol, Bolzano, Italy.
[Montagnani, L.] Autonomous Prov Bolzano, Forest Serv, Bolzano, Italy.
[Marcolla, B.] Fdn Edmund Mach, Sustainable Agroecosyst & Bioresources Dept, I-38010 San Michele All Adige, TN, Italy.
[Toscano, P.] Inst Biometeorol IBIMET CNR, I-50145 Florence, Italy.
[Varlagin, A.] Russian Acad Sci, AN Severtsov Inst Ecol & Evolut, Moscow 119071, Russia.
[Roupsard, O.] CIRAD, UMR Eco&Sols Ecol Fonct & Biogeochim Sols & Agroe, F-34000 Montpellier, France.
[Roupsard, O.] CATIE Trop Agr Ctr Res & Higher Educ, Turrialba 937170, Costa Rica.
[Cescatti, A.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy.
[Arain, M. A.] McMaster Univ, McMaster Ctr Climate Change, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada.
[D'Odorico, P.] ETH, Inst Agr Sci, CH-8092 Zurich, Switzerland.
RP Verma, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Manish.K.Verma@jpl.nasa.gov
RI Montagnani, Leonardo/F-1837-2016; Wohlfahrt, Georg/D-2409-2009; Law,
Beverly/G-3882-2010;
OI Montagnani, Leonardo/0000-0003-2957-9071; Wohlfahrt,
Georg/0000-0003-3080-6702; Law, Beverly/0000-0002-1605-1203; Marcolla,
Barbara/0000-0001-6357-4616; Varlagin, Andrej/0000-0002-2549-5236;
Kiely, Gerard/0000-0003-2189-6427; Toscano, Piero/0000-0001-9184-0707
FU NASA [NNX11AE75G]; National Science Foundation Macrosystem Biology
program [EF-1065029]; AmeriFlux [the Office of Science (BER), US
Department of Energy (DOE)] [DE-FG02-04ER63917, DE-FG02-04ER63911];
AmeriFlux (U.S. Department of Energy, Biological and Environmental
Research, Terrestrial Carbon Program) [DE-FG02-04ER63917,
DE-FG02-04ER63911]; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan;
CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for
Biogeochemistry; National Science Foundation; University of Tuscia;
Universite Laval; US Department of Energy
FX This research was partially supported by NASA grant number NNX11AE75G,
the National Science Foundation Macrosystem Biology program (award
EF-1065029), and AmeriFlux [the Office of Science (BER), US Department
of Energy (DOE; DE-FG02-04ER63917 and DE-FG02-04ER63911)]. MV and MAF
gratefully acknowledge the efforts of the FLUXNET community to compile
and make available the La Thuile data set. This work used eddy
covariance data acquired by the FLUXNET community and in particular by
the following networks: AmeriFlux (U.S. Department of Energy, Biological
and Environmental Research, Terrestrial Carbon Program
(DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, Asia Flux,
CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, China Flux,
Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada,
and NRCan), Green Grass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, USCCC.
We acknowledge the financial support to the eddy covariance data
harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max
Planck Institute for Biogeochemistry, National Science Foundation,
University of Tuscia, Universite Laval, Environment Canada and US
Department of Energy and the database development and technical support
from Berkeley Water Center, Lawrence Berkeley National Laboratory,
Microsoft Research eScience, Oak Ridge National Laboratory, University
of California Berkeley and the University of Virginia.
NR 82
TC 3
Z9 3
U1 12
U2 57
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD DEC 15
PY 2015
VL 214
BP 416
EP 429
DI 10.1016/j.agrformet.2015.09.005
PG 14
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA CW1DO
UT WOS:000364730000038
ER
PT J
AU Makowski, D
Asseng, S
Ewert, F
Bassu, S
Durand, JL
Li, T
Martre, P
Adam, M
Aggarwal, PK
Angulo, C
Baron, C
Basso, B
Bertuzzi, P
Biernath, C
Boogaard, H
Boote, KJ
Bouman, B
Bregaglio, S
Brisson, N
Buis, S
Cammarano, D
Challinor, AJ
Confalonieri, R
Conijn, JG
Corbeels, M
Deryng, D
De Sanctis, G
Doltra, J
Fumoto, T
Gaydon, D
Gayler, S
Goldberg, R
Grant, RF
Grassini, P
Hatfield, JL
Hasegawa, T
Heng, L
Hoek, S
Hooker, J
Hunt, LA
Ingwersen, J
Izaurralde, RC
Jongschaap, REE
Jones, JW
Kemanian, RA
Kersebaum, KC
Kim, SH
Lizaso, J
Marcaida, M
Muller, C
Nakagawa, H
Kumar, SN
Nendel, C
O'Leary, GJ
Olesen, JE
Oriol, P
Osborne, TM
Palosuo, T
Pravia, MV
Priesack, E
Ripoche, D
Rosenzweig, C
Ruane, AC
Ruget, F
Sau, F
Semenov, MA
Shcherbak, I
Singh, B
Singh, U
Soo, HK
Steduto, P
Stockle, C
Stratonovitch, P
Streck, T
Supit, I
Tang, L
Tao, F
Teixeira, EI
Thorburn, P
Timlin, D
Travasso, M
Rotter, RP
Waha, K
Wallach, D
White, JW
Wilkens, P
Williams, JR
Wolf, J
Yin, X
Yoshida, H
Zhang, Z
Zhu, Y
AF Makowski, D.
Asseng, S.
Ewert, F.
Bassu, S.
Durand, J. L.
Li, T.
Martre, P.
Adam, M.
Aggarwal, P. K.
Angulo, C.
Baron, C.
Basso, B.
Bertuzzi, P.
Biernath, C.
Boogaard, H.
Boote, K. J.
Bouman, B.
Bregaglio, S.
Brisson, N.
Buis, S.
Cammarano, D.
Challinor, A. J.
Confalonieri, R.
Conijn, J. G.
Corbeels, M.
Deryng, D.
De Sanctis, G.
Doltra, J.
Fumoto, T.
Gaydon, D.
Gayler, S.
Goldberg, R.
Grant, R. F.
Grassini, P.
Hatfield, J. L.
Hasegawa, T.
Heng, L.
Hoek, S.
Hooker, J.
Hunt, L. A.
Ingwersen, J.
Izaurralde, R. C.
Jongschaap, R. E. E.
Jones, J. W.
Kemanian, R. A.
Kersebaum, K. C.
Kim, S. -H.
Lizaso, J.
Marcaida, M., III
Mueller, C.
Nakagawa, H.
Kumar, S. Naresh
Nendel, C.
O'Leary, G. J.
Olesen, J. E.
Oriol, P.
Osborne, T. M.
Palosuo, T.
Pravia, M. V.
Priesack, E.
Ripoche, D.
Rosenzweig, C.
Ruane, A. C.
Ruget, F.
Sau, F.
Semenov, M. A.
Shcherbak, I.
Singh, B.
Singh, U.
Soo, H. K.
Steduto, P.
Stoeckle, C.
Stratonovitch, P.
Streck, T.
Supit, I.
Tang, L.
Tao, F.
Teixeira, E. I.
Thorburn, P.
Timlin, D.
Travasso, M.
Roetter, R. P.
Waha, K.
Wallach, D.
White, J. W.
Wilkens, P.
Williams, J. R.
Wolf, J.
Yin, X.
Yoshida, H.
Zhang, Z.
Zhu, Y.
TI A statistical analysis of three ensembles of crop model responses to
temperature and CO2 concentration
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Climate change; Crop model; Emulator; Meta-model; Statistical model;
Yield
ID CLIMATE-CHANGE; WHEAT YIELDS; METAANALYSIS; UNCERTAINTY; SIMULATION;
IMPACTS
AB Ensembles of process-based crop models are increasingly used to simulate crop growth for scenarios of temperature and/or precipitation changes corresponding to different projections of atmospheric CO2 concentrations. This approach generates large datasets with thousands of simulated crop yield data. Such datasets potentially provide new information but it is difficult to summarize them in a useful way due to their structural complexities. An associated issue is that it is not straightforward to compare crops and to interpolate the results to alternative climate scenarios not initially included in the simulation protocols. Here we demonstrate that statistical models based on random-coefficient regressions are able to emulate ensembles of process-based crop models. An important advantage of the proposed statistical models is that they can interpolate between temperature levels and between CO2 concentration levels, and can thus be used to calculate temperature and [CO2] thresholds leading to yield loss or yield gain, without rerunning the original complex crop models. Our approach is illustrated with three yield datasets simulated by 19 maize models, 26 wheat models, and 13 rice models. Several statistical models are fitted to these datasets, and are then used to analyze the variability of the yield response to [CO2] and temperature. Based on our results, we show that, for wheat, a [CO2] increase is likely to outweigh the negative effect of a temperature increase of +2 degrees C in the considered sites. Compared to wheat, required levels of [CO2] increase are much higher for maize, and intermediate for rice. For all crops, uncertainties in simulating climate change impacts increase more with temperature than with elevated [CO2]. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Makowski, D.; Bassu, S.; Brisson, N.] INRA, UMR Agron INRA AgroParisTech 211, F-78850 Thiverval Grignon, France.
[Asseng, S.; Jones, J. W.] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA.
[Ewert, F.; Angulo, C.] Univ Bonn, Inst Crop Sci & Resource Conservat INRES, D-53115 Bonn, Germany.
[Durand, J. L.] INRA, Unite Rech Pluridisciplinaire Prairie & Plantes F, F-86600 Lusignan, France.
[Li, T.; Bouman, B.; Marcaida, M., III] Int Rice Res Inst, Los Banos, Philippines.
[Martre, P.] INRA, Genet Divers & Ecophysiol Cererals GDEC UMR1095, F-63100 Clermont Ferrand, France.
[Martre, P.] Blaise Pascal Univ, GDEC UMR1095, F-63170 Aubiere, France.
[Adam, M.; Oriol, P.] CIRAD, UMR AGAP PAM, Montpellier, France.
[Aggarwal, P. K.] Int Water Management Inst, CGIAR Res Program Climate Change Agr & Food Secur, New Delhi 110012, India.
[Baron, C.] CIRAD, UMR TETIS, F-34093 Montpellier, France.
[Basso, B.; Shcherbak, I.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48823 USA.
[Basso, B.; Shcherbak, I.] Michigan State Univ, WK Kellogg Biol Stn, E Lansing, MI 48823 USA.
[Bertuzzi, P.; Brisson, N.; Ripoche, D.] INRA, AgroClim US1116, F-84914 Avignon, France.
[Biernath, C.; Priesack, E.] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Soil Ecol, D-85764 Neuherberg, Germany.
[Boogaard, H.; Hoek, S.] Alterra, Ctr Geoinformat, NL-6700 AA Wageningen, Netherlands.
[Boote, K. J.] Univ Florida, Dept Agron, Gainesville, FL 32611 USA.
[Bregaglio, S.; Confalonieri, R.] Univ Milan, Cassandra Lab, Milan, Italy.
[Buis, S.; Ruget, F.] INRA, EMMAH UMR1114, F-84914 Avignon, France.
[Challinor, A. J.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Challinor, A. J.] Int Ctr Trop Agr CIAT, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia.
[Conijn, J. G.] Univ Wageningen & Res Ctr, WUR Plant Res Int, NL-6708 PB Wageningen, Netherlands.
[Corbeels, M.; Jongschaap, R. E. E.] CIRAD, Agroecol & Sustainable Intensificat Annual Crops, F-34398 Montpellier 5, France.
[Corbeels, M.; Jongschaap, R. E. E.] Embrapa Cerrados, BR-73301970 Planaltina, DF, Brazil.
[Deryng, D.] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England.
[Deryng, D.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Doltra, J.] Cantabria Govt, Cantabrian Agr Res & Training Ctr CIFA, Muriedas 39600, Spain.
[Fumoto, T.; Hasegawa, T.] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan.
[Gaydon, D.] CSIRO Agr Flagship, Dutton Pk, Qld 4102, Australia.
[Gayler, S.] Univ Tubingen, WESS Water & Earth Syst Sci Competence Cluster, D-72074 Tubingen, Germany.
[Goldberg, R.; Rosenzweig, C.; Ruane, A. C.] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Grant, R. F.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2E3, Canada.
[Li, T.; Bouman, B.; Marcaida, M., III] Univ Nebraska, Dept Agron & Hort, Lincoln, NE 68503 USA.
[Hatfield, J. L.] Natl Lab Agr & Environm, Ames, IA 50011 USA.
[Heng, L.] IAEA, A-1400 Vienna, Austria.
[Hooker, J.] Univ Reading, Dept Agr, Reading RG6 6AR, Berks, England.
[Hunt, L. A.] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada.
[Ingwersen, J.; Streck, T.] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany.
[Izaurralde, R. C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Kemanian, R. A.; Pravia, M. V.] INIA, Treinta Y Tres 33000, Uruguay.
[Kersebaum, K. C.; Nendel, C.] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany.
[Kim, S. -H.] Univ Washington, Coll Environm, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
[Lizaso, J.] Univ Politecn Madrid, Dept Prod Vegetal, Fitotecnia, E-28040 Madrid, Spain.
[Mueller, C.; Waha, K.] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Nakagawa, H.; Yoshida, H.] Natl Agr & Food Res Org, Tokyo, Japan.
[Kumar, S. Naresh] IARI PUSA, Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India.
[O'Leary, G. J.] Grains Innovat Pk, Dept Econ Dev Jobs Transport & Resources, Horsham, Vic 3400, Australia.
[Olesen, J. E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark.
[Osborne, T. M.] Univ Reading, Walker Inst, NCAS Climate, Reading RG6 6BB, Berks, England.
[Pravia, M. V.] Penn State Univ, Dept Plant Sci, University Pk, PA 16802 USA.
[Ruget, F.] UAPV, EMMAH UMR1114, F-84914 Avignon, France.
[Sau, F.] Univ Politecn Madrid, Dept Biol Vegetal, E-28040 Madrid, Spain.
[Semenov, M. A.; Stratonovitch, P.] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England.
[Singh, U.; Wilkens, P.] Int Fertilizer Dev Inst, Florence, AL USA.
[Soo, H. K.] Univ Washington, Coll Environm, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
[Steduto, P.] FAO, I-00100 Rome, Italy.
[Stoeckle, C.] Washington State Univ, Biol Syst Engn, Pullman, WA 99164 USA.
[Supit, I.; Wolf, J.] Wageningen Univ, Plant Prod Syst & Earth Syst Sci, NL-6700 AA Wageningen, Netherlands.
[Tang, L.; Zhu, Y.] Nanjing Agr Univ, Natl Engn & Technol Ctr Informat Agr, Nanjing, Jiangsu, Peoples R China.
[Palosuo, T.; Tao, F.; Roetter, R. P.] Nat Resources Inst Finland Luke, FI-00790 Helsinki, Finland.
[Teixeira, E. I.] New Zealand Inst Plant & Food Res Ltd, Sustainable Prod, Canterbury, New Zealand.
[Thorburn, P.] CSIRO Agr Flagship, Dutton Pk, Qld 4102, Australia.
[Timlin, D.] ARS, USDA, Crop Syst & Global Change Lab, Beltsville, MD 20705 USA.
[Travasso, M.] INTA CIRN, Inst Climate & Water, RA-1712 Castelar, Argentina.
[Izaurralde, R. C.; Wallach, D.] INRA, UMR Agrosyst & Dev Territorial AGIR 1248, F-31326 Castanet Tolosan, France.
[White, J. W.] Arid Land Agr Res Ctr, Maricopa, AZ 85138 USA.
[Williams, J. R.] Texas A&M Univ, Texas AgriLife Res & Extens, College Stn, TX 77843 USA.
[Yin, X.] Wageningen Univ, Ctr Crop Syst Anal, NL-6700 AP Wageningen, Netherlands.
[Zhang, Z.] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China.
[Cammarano, D.] James Hutton Inst Invergowrie, Dundee DD2 5DA, Scotland.
[Waha, K.] CSIRO Agr, St Lucia, Qld 4067, Australia.
[De Sanctis, G.] Commiss European Communities, Joint Res Ctr, I-21027 Ispra, Italy.
[Singh, B.] CIMMYT India, New Delhi 110008, India.
RP Makowski, D (reprint author), INRA, UMR Agron INRA AgroParisTech 211, F-78850 Thiverval Grignon, France.
EM makowski@grignon.inra.fr; sasseng@ufl.edu; fewert@uni-bonn.de;
jean-louis.durand@lusignan.inra.fr; t.li@irri.org;
pierre.martre@clermont.inra.fr; p.k.aggarwal@cigar.org;
klav@uni-bonn.de; basso@msu.edu; dominique.ripoche@avignon.inra.fr;
priesack@helmholtz-muenchen.de; kjboote@ufl.edu;
simone.bregaglio@unimi.it; patrick.bertuzzi@avignon.inra.fr;
davide.cammarano@hutton.ac.uk; a.j.challinor@leeds.ac.uk;
roberto.confalonieri@unimi.it; sjaak.conijn@wur.nl; corbeels@cirad.fr;
giacomo.de-sanctis@jrc.ec.europa.eu; jordidoltra@cifacantabria.org;
Don.Gaydon@csiro.au; Sebastian.gayler@uni-tuebingen.de;
cynthia.rosenzweig@nasa.gov; rgrant@ualberta.ca;
jerry.hatfield@ars.usda.gov; L.Heng@iaea.org; j.hooker@reading.ac.uk;
thunt@uoguelph.ca; joachim.ingwersen@uni-hohenheim.de; cizaurra@umd.edu;
sjaak.conijn@wur.nl; jimj@ufl.edu; vpravia@inia.org.uy;
ckersebaum@zalf.de; christoph.mueller@pik-potsdam.de;
nareshkumar.soora@gmail.com; nendel@zalf.de;
garry.O'leary@ecodev.vic.gov.au; jeo@agro.au.dk;
t.m.osborne@reading.ac.uk; taru.palosuo@luke.fi;
christian.biernath@helmholtz-muenchen.de; ccrag1@yahoo.com;
alexander.c.ruane@nasa.gov; mikhail.semenov@rothamsted.ac.uk;
shcherba@mail.msu.edu; Balwinder.singh@cgiar.org;
Pasquale.Steduto@fao.org; stockle@wsu.edu;
pierre.stratonovitch@rothamsted.ac.uk; tstreck@uni-hohenheim.de;
iwan.supit@wur.nl; tangl@njau.edu.cn; fulu.tao@luke.fi;
Edmar.teixeira@plantandfood.co.nz; peter.thorburn@csiro.au;
mtravasso@cnia.inta.gov.ar; reimund.rotter@luke.fi;
katharina.waha@csiro.au; daniel.wallach@toulouse.inra.fr;
jeffrey.white@ars.usda.gov; jwilliams@brc.tamus.edu; joost.wolf@wur.nl;
yanzhu@njau.edu.cn
RI Deryng, Delphine/F-7417-2010; De Sanctis, Giacomo/F-3498-2017; Palosuo,
Taru/B-9593-2012; Doltra, Jordi/C-2106-2015; Gaydon, Donald
/F-4608-2012; Thorburn, Peter/A-6884-2011; Priesack, Eckart/M-7341-2014;
Martre, Pierre/G-5399-2013; Teixeira, Edmar/K-1238-2016; Mueller,
Christoph/E-4812-2016; YADAV, SUDHIR/K-7110-2012; Kim,
Soo-Hyung/A-3012-2009; Singh, Balwinder/F-3063-2011; Olesen,
Jorgen/C-2905-2016; Challinor, Andrew/C-4992-2008
OI Deryng, Delphine/0000-0001-6214-7241; De Sanctis,
Giacomo/0000-0002-3527-8091; Grant, Robert/0000-0002-8890-6231; Boote,
Kenneth/0000-0002-1358-5496; Kersebaum, Kurt
Christian/0000-0002-3679-8427; Priesack, Eckart/0000-0002-5088-9528;
Palosuo, Taru/0000-0003-4322-3450; Martre, Pierre/0000-0002-7419-6558;
Teixeira, Edmar/0000-0002-4835-0590; Mueller,
Christoph/0000-0002-9491-3550; YADAV, SUDHIR/0000-0001-7658-8144; Kim,
Soo-Hyung/0000-0003-3879-4080; Singh, Balwinder/0000-0002-6715-2207;
Olesen, Jorgen/0000-0002-6639-1273; Challinor,
Andrew/0000-0002-8551-6617
FU Victorian Department of Economic Development Jobs, Transport and
Resources; Australian Department of Agriculture; INRA ACCAF
meta-program; Ministry of Science, Research and Arts of
Baden-Wurttemberg [AZ Zu33-721.3-2]; Helmholtz Centre for Environmental
Research - UFZ, Leipzig; FACCE MACSUR project by Innovation Fund
Denmark; FACCE MACSUR project through the German Federal Ministry of
Education and Research [031A103B, 2812ERA115]; Helmholtz project
'REKLIMRegional Climate Change: Causes and Effects' Topic 5:
'Chemistry-climate interactions on global to regional scales'; Royal
Society of New Zealand; Climate Change Impacts and Implications for New
Zealand (CCII) project; Texas AgriLife Research and Extension, Texas AM
University; USDA National Institute for Food and Agriculture
[32011-680002-30191]; FACCE MACSUR project by the German Ministry for
Education and Research (BMBF) [031A103B]; FACE MACSUR project through
the German Federal Office for Agriculture and Food [2812ERA147]; BMBF
via the CARBIOCIAL research project [01LL0902M]; National High-Tech
Research and Development Program of China [2013AA100404]; Priority
Academic Program Development of Jiangsu Higher Education Institutions in
China (PAPD)
FX G.J. O'Leary was supported by the Victorian Department of Economic
Development Jobs, Transport and Resources, the Australian Department of
Agriculture. S. Bassu, P. Bertuzzi, G. De Sanctis, J.-L. Durand, D.
Makowski, P. Martre, D. Ripoche and D. Wallach were partly supported by
the INRA ACCAF meta-program. S. Gayler was supported by a grant from the
Ministry of Science, Research and Arts of Baden-Wurttemberg (AZ
Zu33-721.3-2) and the Helmholtz Centre for Environmental Research - UFZ,
Leipzig. J. E. Olesen was funded through the FACCE MACSUR project by
Innovation Fund Denmark. F. Ewert and C. Angulo received support from
the FACCE MACSUR project (031A103B) funded through the German Federal
Ministry of Education and Research (2812ERA115). C. Biernath was funded
through the Helmholtz project 'REKLIMRegional Climate Change: Causes and
Effects' Topic 5: 'Chemistry-climate interactions on global to regional
scales'. EI Teixeira was supported by the Royal Society of New Zealand
and the Climate Change Impacts and Implications for New Zealand (CCII)
project. R. C. Izaurralde and J. R. Williams were funded by Texas
AgriLife Research and Extension, Texas A&M University. C. O. Stockle was
funded through USDA National Institute for Food and Agriculture award
32011-680002-30191. C. Muller was funded through the FACCE MACSUR
project by the German Ministry for Education and Research (BMBF,
031A103B). K.C. Kersebaum and C. Nendel were supported by FACE MACSUR
project funded through the German Federal Office for Agriculture and
Food (2812ERA147). C. Nendel received support by BMBF via the CARBIOCIAL
research project (01LL0902M).r Y. Zhu and L. Tang were supported by the
National High-Tech Research and Development Program of China
(2013AA100404) and the Priority Academic Program Development of Jiangsu
Higher Education Institutions in China (PAPD).
NR 17
TC 3
Z9 3
U1 24
U2 86
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD DEC 15
PY 2015
VL 214
BP 483
EP 493
DI 10.1016/j.agrformet.2015.09.013
PG 11
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA CW1DO
UT WOS:000364730000043
ER
PT J
AU Masnovi, J
Banger, KK
Fanwick, PE
Hepp, AF
AF Masnovi, John
Banger, Kulbinder K.
Fanwick, Philip E.
Hepp, Aloysius F.
TI Structural characterization of copper-indium chalcopyrite precursors
(PPh3)(2)CuIn(ER)(4) [R = CH3, E = S and R = Ph, E = S and Se]
SO POLYHEDRON
LA English
DT Article
DE Copper; Indium; Chalcopyrite; Precursors; Photovoltaics
ID SINGLE-SOURCE PRECURSORS; THIN-FILM; SOLAR-CELLS; CUINS2; COMPLEXES;
CLUSTER
AB Three copper-indium bimetallic compounds, (PPh3)(2)CuIn(ER)(4) [R= CH3, E = S and R = Ph, E = S and Se], potentially useful as single-source precursors for the lower temperature (<400 degrees C) synthesis of ternary chalcopyrite photovoltaic materials, contain an inorganic core structure consisting of two triphenylphosphine ligands attached to Cu(I), two thiolate or selenolate ligands attached to In(III), and an additional two bridging S or Se anion ligands. The metal and bridging chalcogen atoms form planar rings. The ligands adopt geometries to minimize steric interactions, and the intramolecular Cu center dot center dot center dot In nonbonded distances (3.285-3.500 angstrom) depend on the stereoelectronic demands of the ligands. Published by Elsevier Ltd.
C1 [Masnovi, John] Cleveland State Univ, Dept Chem, Cleveland, OH 44115 USA.
[Banger, Kulbinder K.] Ohio Aerosp Inst, Brookpark, OH 44142 USA.
[Fanwick, Philip E.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Hepp, Aloysius F.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hepp, AF (reprint author), NASA Glenn Res Ctr, MS 302-1,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM j.masnovi@csuohio.edu; kkb_28@yahoo.com; pfanwick@purdue.edu;
Aloysius.F.Hepp@nasa.gov
FU NASA Glenn Research Center (GRC) at Lewis Field; NASA GRC [NCC3-710,
NCC3-817, NCC3-947, NCC-958]; Faculty Fellowship Program
FX The authors would like to thank NASA Glenn Research Center (GRC) at
Lewis Field for support of this work. KKB acknowledges NASA GRC funding
of Cooperative Agreements NCC3-710, NCC3-817, NCC3-947, and NCC-958; JM
is grateful for NASA GRC support through the Faculty Fellowship Program.
NR 25
TC 2
Z9 2
U1 2
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-5387
J9 POLYHEDRON
JI Polyhedron
PD DEC 14
PY 2015
VL 102
BP 246
EP 252
DI 10.1016/j.poly.2015.09.038
PG 7
WC Chemistry, Inorganic & Nuclear; Crystallography
SC Chemistry; Crystallography
GA DA4GC
UT WOS:000367757100032
ER
PT J
AU Mackie, CJ
Candian, A
Huang, XC
Maltseva, E
Petrignani, A
Oomens, J
Buma, WJ
Lee, TJ
Tielens, AGGM
AF Mackie, Cameron J.
Candian, Alessandra
Huang, Xinchuan
Maltseva, Elena
Petrignani, Annemieke
Oomens, Jos
Buma, Wybren Jan
Lee, Timothy J.
Tielens, Alexander G. G. M.
TI The anharmonic quartic force field infrared spectra of three polycyclic
aromatic hydrocarbons: Naphthalene, anthracene, and tetracene
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID VIBRATIONAL-SPECTRA; PERTURBATION-THEORY; EMISSION FEATURES; FERMI
RESONANCE; SPECTROSCOPY; IR; BANDS; MOLECULES; GRAPHENE; DATABASE
AB Current efforts to characterize and study interstellar polycyclic aromatic hydrocarbons (PAHs) rely heavily on theoretically predicted infrared (IR) spectra. Generally, such studies use the scaled harmonic frequencies for band positions and double harmonic approximation for intensities of species, and then compare these calculated spectra with experimental spectra obtained under matrix isolation conditions. High-resolution gas-phase experimental spectroscopic studies have recently revealed that the double harmonic approximation is not sufficient for reliable spectra prediction. In this paper, we present the anharmonic theoretical spectra of three PAHs: naphthalene, anthracene, and tetracene, computed with a locally modified version of the SPECTRO program using Cartesian derivatives transformed from Gaussian 09 normal coordinate force constants. Proper treatments of Fermi resonances lead to an impressive improvement on the agreement between the observed and theoretical spectra, especially in the C-H stretching region. All major IR absorption features in the full-scale matrix-isolated spectra, the high-temperature gas-phase spectra, and the most recent high-resolution gas-phase spectra obtained under supersonically cooled molecular beam conditions in the CH-stretching region are assigned. (C) 2015 AIP Publishing LLC.
C1 [Mackie, Cameron J.; Candian, Alessandra; Petrignani, Annemieke; Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Maltseva, Elena; Buma, Wybren Jan] Univ Amsterdam, NL-1098 XH Amsterdam, Netherlands.
[Petrignani, Annemieke; Oomens, Jos] Radboud Univ Nijmegen, FELIX Lab, NL-6525 ED Nijmegen, Netherlands.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mackie, CJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM mackie@strw.leidenuniv.nl
RI Lee, Timothy/K-2838-2012; Oomens, Jos/F-9691-2015; Buma, Wybren
Jan/F-6691-2011; HUANG, XINCHUAN/A-3266-2013;
OI Buma, Wybren Jan/0000-0002-1265-8016; Mackie,
Cameron/0000-0003-2885-2021; Petrignani, Annemieke/0000-0002-6116-5867;
Candian, Alessandra/0000-0002-5431-4449
FU Advanced European Research Council [246976]; Spinoza award; Dutch
Astrochemistry Network - Netherlands Organization for Scientific
Research, NWO; NWO Exacte Wetenschappen [MP-270-13, MP-264-14]; NASA
[12-APRA12-0107]; NASA/SETI [NNX12AG96A, NNX15AF45A]; National
Aeronautics and Space Administration through the NASA Astrobiology
Institute through the Science Mission Directorate [NNH13ZDA017C]
FX The authors would like to thank the two anonymous reviewers for their
helpful comments that improved the clarity of the manuscript. The
spectroscopic study of interstellar PAHs at Leiden Observatory has been
supported through the Advanced European Research Council Grant No.
246976, a Spinoza award, and through the Dutch Astrochemistry Network
funded by the Netherlands Organization for Scientific Research, NWO.
Computing time has been made available by NWO Exacte Wetenschappen
(Project Nos. MP-270-13 and MP-264-14) and calculations were performed
at the LISA Linux cluster of the SurfSARA supercomputer center in
Almere, The Netherlands. X.H. and T.J.L. gratefully acknowledge support
from the NASA No. 12-APRA12-0107 grant. X.H. acknowledges the support
from NASA/SETI Co-op Agreement Nos. NNX12AG96A and NNX15AF45A. This
material is based upon work supported by the National Aeronautics and
Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice No. NNH13ZDA017C issued through the Science
Mission Directorate. A.C. acknowledges Fernando Clemente and Julien
Bloino for insightful discussions.
NR 49
TC 6
Z9 6
U1 9
U2 24
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 DEC 14
PY 2015
VL 143
IS 22
AR 224314
DI 10.1063/1.4936779
PG 15
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CZ6EP
UT WOS:000367194300034
PM 26671382
ER
PT J
AU Saro, A
Bocquet, S
Rozo, E
Benson, BA
Mohr, J
Rykoff, ES
Soares-Santos, M
Bleem, L
Dodelson, S
Melchior, P
Sobreira, F
Upadhyay, V
Weller, J
Abbott, T
Abdalla, FB
Allam, S
Armstrong, R
Banerji, M
Bauer, AH
Bayliss, M
Benoit-Levy, A
Bernstein, GM
Bertin, E
Brodwin, M
Brooks, D
Buckley-Geer, E
Burke, DL
Carlstrom, JE
Capasso, R
Capozzi, D
Rosell, AC
Kind, MC
Chiu, I
Covarrubias, R
Crawford, TM
Crocce, M
D'Andrea, CB
da Costa, LN
DePoy, DL
Desai, S
de Haan, T
Diehl, HT
Dietrich, JP
Doel, P
Cunha, CE
Eifler, TF
Evrard, AE
Neto, AF
Fernandez, E
Flaugher, B
Fosalba, P
Frieman, J
Gangkofner, C
Gaztanaga, E
Gerdes, D
Gruen, D
Gruendl, RA
Gupta, N
Hennig, C
Holzapfel, WL
Honscheid, K
Jain, B
James, D
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Lin, H
Maia, MAG
March, M
Marshall, JL
Martini, P
McDonald, M
Miller, CJ
Miquel, R
Nord, B
Ogando, R
Plazas, AA
Reichardt, CL
Romer, AK
Roodman, A
Sako, M
Sanchez, E
Schubnell, M
Sevilla, I
Smith, RC
Stalder, B
Stark, AA
Strazzullo, V
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Tucker, D
Vikram, V
von der Linden, A
Walker, AR
Wechsler, RH
Wester, W
Zenteno, A
Ziegler, KE
AF Saro, A.
Bocquet, S.
Rozo, E.
Benson, B. A.
Mohr, J.
Rykoff, E. S.
Soares-Santos, M.
Bleem, L.
Dodelson, S.
Melchior, P.
Sobreira, F.
Upadhyay, V.
Weller, J.
Abbott, T.
Abdalla, F. B.
Allam, S.
Armstrong, R.
Banerji, M.
Bauer, A. H.
Bayliss, M.
Benoit-Levy, A.
Bernstein, G. M.
Bertin, E.
Brodwin, M.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Carlstrom, J. E.
Capasso, R.
Capozzi, D.
Carnero Rosell, A.
Kind, M. Carrasco
Chiu, I.
Covarrubias, R.
Crawford, T. M.
Crocce, M.
D'Andrea, C. B.
da Costa, L. N.
DePoy, D. L.
Desai, S.
de Haan, T.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Cunha, C. E.
Eifler, T. F.
Evrard, A. E.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Gerdes, D.
Gruen, D.
Gruendl, R. A.
Gupta, N.
Hennig, C.
Holzapfel, W. L.
Honscheid, K.
Jain, B.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Lin, H.
Maia, M. A. G.
March, M.
Marshall, J. L.
Martini, Paul
McDonald, M.
Miller, C. J.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A. A.
Reichardt, C. L.
Romer, A. K.
Roodman, A.
Sako, M.
Sanchez, E.
Schubnell, M.
Sevilla, I.
Smith, R. C.
Stalder, B.
Stark, A. A.
Strazzullo, V.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D.
Vikram, V.
von der Linden, A.
Walker, A. R.
Wechsler, R. H.
Wester, W.
Zenteno, A.
Ziegler, K. E.
TI Constraints on the richness-mass relation and the optical-SZE positional
offset distribution for SZE-selected clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE catalogues; methods: data analysis; galaxies: abundances; galaxies:
clusters: general; galaxies: haloes; galaxies: statistics; cosmology:
miscellaneous; large-scale structure of Universe
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; SCIENCE VERIFICATION DATA;
BLANCO COSMOLOGY SURVEY; 720 SQUARE DEGREES; X-RAY-PROPERTIES;
SIMILAR-TO 1; GALAXY CLUSTERS; SCALING RELATIONS; DATA RELEASE
AB We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg(2) of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 less than or similar to z less than or similar to 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness lambda-mass relation with the following function < ln lambda| M-500 > alpha B-lambda ln M-500 + C(lambda)ln E(z) and use SPT-SZ cluster masses and RM richnesses lambda to constrain the parameters. We find B-lambda = 1.14(-0.18)(+0.21) and C-lambda = 0.73(-0.75)(+0.77). The associated scatter in mass at fixed richness is sigma M-ln|lambda = 0.18(-0.05)(+0.08) at a characteristic richness lambda= 70. We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RM-selected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RM catalogue with SPT-SZ candidates below the official catalogue threshold significance xi = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with xi is an element of [4, 4.5].
C1 [Saro, A.; Bocquet, S.; Mohr, J.; Capasso, R.; Chiu, I.; Desai, S.; Dietrich, J. P.; Gangkofner, C.; Gupta, N.; Hennig, C.; Strazzullo, V.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Saro, A.; Bocquet, S.; Mohr, J.; Weller, J.; Capasso, R.; Chiu, I.; Dietrich, J. P.; Gangkofner, C.; Gupta, N.; Hennig, C.; Strazzullo, V.] Excellence Cluster Univ, D-85748 Garching, Germany.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Benson, B. A.; Soares-Santos, M.; Dodelson, S.; Sobreira, F.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Lin, H.; Nord, B.; Tucker, D.; Wester, W.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Benson, B. A.; Bleem, L.; Dodelson, S.; Carlstrom, J. E.; Crawford, T. M.; Frieman, J.; Ziegler, K. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Dodelson, S.; Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Mohr, J.; Weller, J.; Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Rykoff, E. S.; Burke, D. L.; Cunha, C. E.; Roodman, A.; von der Linden, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Rykoff, E. S.; Burke, D. L.; Roodman, A.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Bleem, L.; Vikram, V.] Argonne Natl Lab, Lemont, IL 60439 USA.
[Melchior, P.; Honscheid, K.; Martini, Paul; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Melchior, P.; Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Sobreira, F.; Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.] Lab Interinst & Astron LIneA, BR-20921400 Rio De Janeiro, Brazil.
[Upadhyay, V.] CERN, CH-1211 Geneva 23, Switzerland.
[Weller, J.; Gruen, D.] Univ Munich, Fak Phys, Univ Sternwarte, D-81679 Munich, Germany.
[Abbott, T.; James, D.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile.
[Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England.
[Armstrong, R.; Bernstein, G. M.; Eifler, T. F.; Jain, B.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Banerji, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Bauer, A. H.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Fac Ciencias, E-08193 Barcelona, Spain.
[Bayliss, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bayliss, M.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bertin, E.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Bertin, E.] CNRS, UMR7095, F-75014 Paris, France.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Capozzi, D.; D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Kind, M. Carrasco; Gruendl, R. A.; Sevilla, I.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Covarrubias, R.; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 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.
[de Haan, T.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[de Haan, T.; Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Evrard, A. E.; Gerdes, D.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Fernandez, E.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Martini, Paul] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla, I.] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
[Stalder, B.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[von der Linden, A.; Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Zenteno, A.] Cerro Tololo Interamer Observ, La Serena, Chile.
RP Saro, A (reprint author), Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany.
EM saro@usm.lmu.de
RI Sobreira, Flavia/F-4168-2015; Ogando, Ricardo/A-1747-2010; Sanchez,
Eusebio/H-5228-2015; Fosalba Vela, Pablo/I-5515-2016;
OI Sobreira, Flavia/0000-0002-7822-0658; CRAWFORD,
THOMAS/0000-0001-9000-5013; Dietrich, Jorg/0000-0002-8134-9591; Weller,
Jochen/0000-0002-8282-2010; Ogando, Ricardo/0000-0003-2120-1154;
Sanchez, Eusebio/0000-0002-9646-8198; Carrasco Kind,
Matias/0000-0002-4802-3194; Stern, Corvin/0000-0003-4406-6127; Abdalla,
Filipe/0000-0003-2063-4345; Tucker, Douglas/0000-0001-7211-5729; Stark,
Antony/0000-0002-2718-9996
FU DFG Cluster of Excellence 'Origin and Structure of the Universe';
Transregio program TR33 'The Dark Universe'; Ludwig-Maximilians
University; National Science Foundation [PLR-1248097]; NSF Physics
Frontier Center [PHY-1125897]; Gordon and Betty Moore Foundation [GBMF
947]; Smithsonian Institution; Miller Research Fellowship; Danish
National Research Foundation; Australian Research Council's Discovery
Projects scheme [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 University
of Chicago; Center for Cosmology and Astro-Particle Physics at 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
and the Ministerio da Ciencia e Tecnologia; Deutsche
Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy
Survey; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de
Excelencia Severo Ochoa [SEV-2012-0234]; European Union
FX We acknowledge the support by the DFG Cluster of Excellence 'Origin and
Structure of the Universe', the Transregio program TR33 'The Dark
Universe' and the Ludwig-Maximilians University. 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. AAS acknowledges a
Pell grant from the Smithsonian Institution. TDH is supported by a
Miller Research Fellowship. This work was partially completed at
Fermilab, operated by Fermi Research Alliance, LLC under contract no.
De-AC02-07CH11359 with the United States Department of Energy. The Dark
Cosmology Centre is funded by the Danish National Research Foundation.
CR acknowledges support from the Australian Research Council's Discovery
Projects scheme (DP150103208). 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 e Tecnologia, the
Deutsche Forschungsgemeinschaft and the Collaborating Institutions in
the Dark Energy Survey. 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, some of which include ERDF funds from the European Union.
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 Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, 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 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.
NR 79
TC 11
Z9 11
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 DEC 11
PY 2015
VL 454
IS 3
BP 2305
EP 2319
DI 10.1093/mnras/stv2141
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7QY
UT WOS:000368000400004
ER
PT J
AU Eifler, T
Krause, E
Dodelson, S
Zentner, AR
Hearin, AP
Gnedin, NY
AF Eifler, Tim
Krause, Elisabeth
Dodelson, Scott
Zentner, Andrew R.
Hearin, Andrew P.
Gnedin, Nickolay Y.
TI Accounting for baryonic effects in cosmic shear tomography: determining
a minimal set of nuisance parameters using PCA
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmological parameters; cosmology: theory; large-scale structure of
Universe
ID MATTER POWER SPECTRUM; WEAK-LENSING SURVEYS; PHOTOMETRIC REDSHIFT
ERRORS; LARGE-SCALE STRUCTURE; DARK-MATTER; COSMOLOGICAL CONSTRAINTS;
GALAXY FORMATION; COYOTE UNIVERSE; NUMBER DENSITY; MASS FUNCTION
AB Systematic uncertainties that have been subdominant in past large-scale structure (LSS) surveys are likely to exceed statistical uncertainties of current and future LSS data sets, potentially limiting the extraction of cosmological information. Here we present a general framework (Principal Component Analysis - PCA - marginalization) to consistently incorporate systematic effects into a likelihood analysis. This technique naturally accounts for degeneracies between nuisance parameters and can substantially reduce the dimension of the parameter space that needs to be sampled. As a practical application, we apply PCA marginalization to account for baryonic physics as an uncertainty in cosmic shear tomography. Specifically, we use COSMOLIKE to run simulated likelihood analyses on three independent sets of numerical simulations, each covering a wide range of baryonic scenarios differing in cooling, star formation, and feedback mechanisms. We simulate a Stage III (Dark Energy Survey) and Stage IV (Large Synoptic Survey Telescope/Euclid) survey and find a substantial bias in cosmological constraints if baryonic physics is not accounted for. We then show that PCA marginalization (employing at most three to four nuisance parameters) removes this bias. Our study demonstrates that it is possible to obtain robust, precise constraints on the dark energy equation of state even in the presence of large levels of systematic uncertainty in astrophysical processes. We conclude that the PCA marginalization technique is a powerful, general tool for addressing many of the challenges facing the precision cosmology programme.
C1 [Eifler, Tim] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Eifler, Tim; Krause, Elisabeth] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Krause, Elisabeth] Stanford Univ, Kavli Inst Particle Cosmol & Astrophys, Stanford, CA 94305 USA.
[Dodelson, Scott; Gnedin, Nickolay Y.] Univ Chicago, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Dodelson, Scott; Gnedin, Nickolay Y.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Dodelson, Scott; Hearin, Andrew P.; Gnedin, Nickolay Y.] Fermilab Natl Accelerator Lab, Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Zentner, Andrew R.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Zentner, Andrew R.] Univ Pittsburgh, PITTsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[Hearin, Andrew P.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
RP Eifler, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tim.eifler@jpl.nasa.gov
FU National Science Foundation [1066293, AST 0806367, AST 1108802];
hospitality of the Aspen Center for Physics; US Department of Energy
[DE-FG02-95ER40896]; Pittsburgh Particle physics, Astrophysics, and
Cosmology Center (PITT PACC) at the University of Pittsburgh; Scientific
Discovery through Advanced Computing (SciDAC) programme - US Department
of Energy, Office of Science, Advanced Scientific Computing Research and
High Energy Physics; National Aeronautics and Space Administration
FX This paper is based upon work supported in part by the National Science
Foundation under Grant no. 1066293 and the hospitality of the Aspen
Center for Physics. The work of SD and NYG is supported by the US
Department of Energy, including grant DE-FG02-95ER40896. The work of ARZ
has been funded in part by the Pittsburgh Particle physics,
Astrophysics, and Cosmology Center (PITT PACC) at the University of
Pittsburgh and by the National Science Foundation under grants AST
0806367 and AST 1108802. Support for this work was provided through the
Scientific Discovery through Advanced Computing (SciDAC) programme
funded by the US Department of Energy, Office of Science, Advanced
Scientific Computing Research and High Energy Physics. Part of the
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 11
PY 2015
VL 454
IS 3
BP 2451
EP 2471
DI 10.1093/mnras/stv2000
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7QY
UT WOS:000368000400017
ER
PT J
AU Maund, JR
Arcavi, I
Ergon, M
Eldridge, JJ
Georgy, C
Cenko, SB
Horesh, A
Izzard, RG
Stancliffe, RJ
AF Maund, J. R.
Arcavi, I.
Ergon, M.
Eldridge, J. J.
Georgy, C.
Cenko, S. B.
Horesh, A.
Izzard, R. G.
Stancliffe, R. J.
TI Did the progenitor of SN 2011dh have a binary companion?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; supernovae: individual: 2011dh
ID IIB SUPERNOVA 2011DH; CORE-COLLAPSE SUPERNOVAE; WOLF-RAYET STAR;
SUPERGIANT PROGENITOR; MASS-LOSS; RED SUPERGIANTS; IB SUPERNOVA; 1993J;
IPTF13BVN; SPECTRA
AB We present late-time Hubble Space Telescope ultraviolet (UV) and optical observations of the site of SN 2011dh in the galaxy M51, similar to 1164 days post-explosion. At the supernova (SN) location, we observe a point source that is visible at all wavelengths, which is significantly fainter than the spectral energy distribution (SED) of the yellow supergiant progenitor observed prior to explosion. The previously reported photometry of the progenitor is, therefore, completely unaffected by any sources that may persist at the SN location after explosion. In comparison with the previously reported late-time photometric evolution of SN 2011dh, we find that the light curve has plateaued at all wavelengths. The SED of the late-time source is clearly inconsistent with an SED of stellar origin. Although the SED is bright at UV wavelengths, there is no strong evidence that the late-time luminosity originates solely from a stellar source corresponding to the binary companion, although a partial contribution to the observed UV flux from a companion star cannot be ruled out.
C1 [Maund, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Arcavi, I.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
[Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Ergon, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Eldridge, J. J.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Georgy, C.] Keele Univ, Astrophys Grp, EPSAM, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Cenko, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Horesh, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Izzard, R. G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Stancliffe, R. J.] Argelander Inst Astron, D-53121 Bonn, Germany.
RP Maund, JR (reprint author), Univ Sheffield, Dept Phys & Astron, Hicks Bldg,Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England.
EM j.maund@sheffield.ac.uk
RI Horesh, Assaf/O-9873-2016
OI Horesh, Assaf/0000-0002-5936-1156
FU Royal Society University Research Fellowship; European Research Council
under the European Union [306901]
FX We are very grateful to Anders Jerkstrand for providing us with access
to his late-time model spectra of SN 2011dh. The research of JRM is
supported by a Royal Society University Research Fellowship. CG
acknowledges support from the European Research Council under the
European Union's Seventh Framework Program (FP/2007-2013)/ERC Grant
Agreement No. 306901.
NR 47
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 11
PY 2015
VL 454
IS 3
BP 2580
EP 2585
DI 10.1093/mnras/stv2098
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7QY
UT WOS:000368000400026
ER
PT J
AU Southworth, J
Mancini, L
Tregloan-Reed, J
Novati, SC
Ciceri, S
D'Ago, G
Delrez, L
Dominik, M
Evans, DF
Gillon, M
Jehin, E
Jorgensen, UG
Haugbolle, T
Lendl, M
Arena, C
Barbieri, L
Barbieri, M
Corfini, G
Lopresti, C
Marchini, A
Marino, G
Alsubai, KA
Bozza, V
Bramich, DM
Jaimes, RF
Hinse, TC
Henning, T
Hundertmark, M
Juncher, D
Korhonen, H
Popovas, A
Rabus, M
Rahvar, S
Schmidt, RW
Skottfelt, J
Snodgrass, C
Starkey, D
Surdej, J
Wertz, O
AF Southworth, John
Mancini, L.
Tregloan-Reed, J.
Novati, S. Calchi
Ciceri, S.
D'Ago, G.
Delrez, L.
Dominik, M.
Evans, D. F.
Gillon, M.
Jehin, E.
Jorgensen, U. G.
Haugbolle, T.
Lendl, M.
Arena, C.
Barbieri, L.
Barbieri, M.
Corfini, G.
Lopresti, C.
Marchini, A.
Marino, G.
Alsubai, K. A.
Bozza, V.
Bramich, D. M.
Jaimes, R. Figuera
Hinse, T. C.
Henning, Th.
Hundertmark, M.
Juncher, D.
Korhonen, H.
Popovas, A.
Rabus, M.
Rahvar, S.
Schmidt, R. W.
Skottfelt, J.
Snodgrass, C.
Starkey, D.
Surdej, J.
Wertz, O.
TI Larger and faster: revised properties and a shorter orbital period for
the WASP-57 planetary system from a pro-am collaboration
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: fundamental parameters; stars: individual: WASP-57; planetary
systems
ID TRANSITING EXTRASOLAR PLANETS; HUBBLE-SPACE-TELESCOPE; STELLAR EVOLUTION
DATABASE; HIGH-PRECISION PHOTOMETRY; LIGHT-CURVE; PHYSICAL-PROPERTIES;
TRANSMISSION SPECTRUM; POPULATION SYNTHESIS; ATMOSPHERIC HAZE; CENTRAL
REGION
AB Transits in the WASP-57 planetary system have been found to occur half an hour earlier than expected. We present 10 transit light curves from amateur telescopes, on which this discovery was based, 13 transit light curves from professional facilities which confirm and refine this finding, and high-resolution imaging which show no evidence for nearby companions. We use these data to determine a new and precise orbital ephemeris, and measure the physical properties of the system. Our revised orbital period is 4.5 s shorter than found from the discovery data alone, which explains the early occurrence of the transits. We also find both the star and planet to be larger and less massive than previously thought. The measured mass and radius of the planet are now consistent with theoretical models of gas giants containing no heavy-element core, as expected for the subsolar metallicity of the host star. Two transits were observed simultaneously in four passbands. We use the resulting light curves to measure the planet's radius as a function of wavelength, finding that our data are sufficient in principle but not in practise to constrain its atmospheric properties. We conclude with a discussion of the current and future status of transmission photometry studies for probing the atmospheres of gas-giant transiting planets.
C1 [Southworth, John; Evans, D. F.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Mancini, L.; Ciceri, S.; Henning, Th.; Rabus, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Novati, S. Calchi] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, S. Calchi; D'Ago, G.; Bozza, V.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi; D'Ago, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[D'Ago, G.; Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Delrez, L.; Gillon, M.; Jehin, E.; Lendl, M.; Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Dominik, M.; Jaimes, R. Figuera; Starkey, D.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Jorgensen, U. G.; Haugbolle, T.; Hundertmark, M.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen, Denmark.
[Jorgensen, U. G.; Haugbolle, T.; Hundertmark, M.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Lendl, M.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Arena, C.; Barbieri, L.; Corfini, G.; Lopresti, C.; Marchini, A.; Marino, G.] Unione Astrofili Italiani, Sez Pianeti Extrasolari, Turin, Italy.
[Arena, C.] Grp Astrofili Catanesi, Catania, Italy.
[Barbieri, L.] Assoc Astrofili Bolognesi, Bologna, Italy.
[Barbieri, M.] Univ Atacama, Dept Phys, Copiapo, Chile.
[Lopresti, C.] Ist Spezzino Ric Astron IRAS, La Spezia, Italy.
[Marchini, A.] Univ Siena, DSFTA Astron Observ, I-53100 Siena, Italy.
[Marino, G.] GAC, Catania, Italy.
[Alsubai, K. A.; Bramich, D. M.] Qatar Environm & Energy Res Inst, Qatar Fdn, Doha 5825, Qatar.
[Jaimes, R. Figuera] European So Observ, D-85748 Garching, Germany.
[Hinse, T. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
[Korhonen, H.] Univ Turku, ESO, FINCA, Finnish Ctr Astron, FI-21500 Piikkio, Finland.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran 111559161, Iran.
[Schmidt, R. W.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany.
[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.
RP Southworth, J (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM astro.js@keele.ac.uk
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; Barbieri,
Mauro/0000-0001-8362-3462; Dominik, Martin/0000-0002-3202-0343; D'Ago,
Giuseppe/0000-0001-9697-7331; Snodgrass, Colin/0000-0001-9328-2905
FU Danish Natural Science Research Council (FNU); ESO La Silla, Chile
[093.A-9007(A)]; Max-Planck Institut fur Astronomie; Instituto de
Astrofisica de Andalucia (CSIC); Belgian Fund for Scientific Research
(Fond National de la Recherche Scientifique, FNRS) [FRFC 2.5.594.09.F];
STFC; Qatar National Research Fund (Qatar Foundation) [NPRP
X-019-1-006]; Korea Astronomy & Space Science Institute [2014-1-400-06];
Korea Astronomy and Space Science Institute (KASI) [2014-1-400-06];
Communaute francaise de Belgique - Actions de recherche concertees -
Academie Wallonie-Europe
FX The operation of the Danish 1.54 m telescope is financed by a grant to
UGJ from the Danish Natural Science Research Council (FNU). This paper
incorporates observations collected using the Gamma Ray Burst Optical
and Near-Infrared Detector (GROND) instrument at the MPG 2.2 m telescope
located at ESO La Silla, Chile, program 093.A-9007(A). GROND was built
by the high-energy group of MPE in collaboration with the LSW Tautenburg
and ESO, and is operated as a PI-instrument at the MPG 2.2 m telescope.
This paper incorporates observations collected at the Centro Astronomico
Hispano Aleman (CAHA) at Calar Alto, Spain, operated jointly by the
Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de
Andalucia (CSIC). TRAPPIST is funded by the Belgian Fund for Scientific
Research (Fond National de la Recherche Scientifique, FNRS) under the
grant FRFC 2.5.594.09.F, with the participation of the Swiss National
Science Fundation (SNF). MG and EJ are FNRS Research Associates. LD is a
FNRS/FRIA Doctoral Fellow. We thank the anonymous referee for a helpful
report and Dr Francesca Faedi for discussions. The reduced light curves
presented in this work will be made available at the CDS
(http://vizier.u-strasbg.fr/) and at
http://www.astro.keele.ac.uk/similar to jkt/. J Southworth acknowledges
financial support from STFC in the form of an Advanced Fellowship. This
publication was partially supported by grant NPRP X-019-1-006 from Qatar
National Research Fund (a member of Qatar Foundation). TCH is supported
by the Korea Astronomy & Space Science Institute travel grant
#2014-1-400-06. TCH acknowledges support from the Korea Astronomy and
Space Science Institute (KASI) grant 2014-1-400-06. OW (FNRS research
fellow) and J Surdej acknowledge support from the Communaute francaise
de Belgique - Actions de recherche concertees - Academie
Wallonie-Europe. The following internet-based resources were used in
research for this paper: the ESO Digitized Sky Survey; the NASA
Astrophysics Data System; the SIMBAD data base and VizieR catalogue
access tool operated at CDS, Strasbourg, France; and the ar chi iv
scientific paper preprint service operated by Cornell University. Based
on data collected by MiNDSTEp with the Danish 1.54 m telescope, and data
collected with GROND on the MPG 2.2 m telescope, both located at ESO La
Silla.
NR 69
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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 DEC 11
PY 2015
VL 454
IS 3
BP 3094
EP 3107
DI 10.1093/mnras/stv2183
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7QY
UT WOS:000368000400064
ER
PT J
AU Middleton, MJ
Walton, DJ
Fabian, A
Roberts, TP
Heil, L
Pinto, C
Anderson, G
Sutton, A
AF Middleton, Matthew J.
Walton, Dominic J.
Fabian, Andrew
Roberts, Timothy P.
Heil, Lucy
Pinto, Ciro
Anderson, Gemma
Sutton, Andrew
TI Diagnosing the accretion flow in ultraluminous X-ray sources using soft
X-ray atomic features
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; X-rays: binaries
ID MASS BLACK-HOLE; HOLMBERG II X-1; NGC 1313 X-1; XMM-NEWTON; BROAD-BAND;
SOLAR MASSES; UPPER LIMITS; NUSTAR; GALAXY; STATE
AB The lack of unambiguous detections of atomic features in the X-ray spectra of ultraluminous X-ray sources (ULXs) has proven a hindrance in diagnosing the nature of the accretion flow. The possible association of spectral residuals at soft energies with atomic features seen in absorption and/or emission and potentially broadened by velocity dispersion could therefore hold the key to understanding much about these enigmatic sources. Here we show for the first time that such residuals are seen in several sources and appear extremely similar in shape, implying a common origin. Via simple arguments we assert that emission from extreme colliding winds, absorption in a shell of material associated with the ULX nebula and thermal plasma emission associated with star formation are all highly unlikely to provide an origin. Whilst CCD spectra lack the energy resolution necessary to directly determine the nature of the features (i.e. formed of a complex of narrow lines or intrinsically broad lines), studying the evolution of the residuals with underlying spectral shape allows for an important, indirect test for their origin. The ULX NGC 1313 X-1 provides the best opportunity to perform such a test due to the dynamic range in spectral hardness provided by archival observations. We show through highly simplified spectral modelling that the strength of the features (in either absorption or emission) appears to anticorrelate with spectral hardness, which would rule out an origin via reflection of a primary continuum and instead supports a picture of atomic transitions in a wind or nearby material associated with such an outflow.
C1 [Middleton, Matthew J.; Fabian, Andrew; Pinto, Ciro] Inst Astron, Cambridge CB3 0HA, England.
[Walton, Dominic J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walton, Dominic J.] CALTECH, Pasadena, CA 91125 USA.
[Roberts, Timothy P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Heil, Lucy] Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Anderson, Gemma] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Sutton, Andrew] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
RP Middleton, MJ (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM mjm@ast.cam.ac.uk
OI Pinto, Ciro/0000-0003-2532-7379
FU ERC [340442]; ORAU under NASA Postdoctoral programme at the NASA Jet
Propulsion Laboratory; STFC [ST/L00075X/1]; ESA Member States; NASA
FX The authors thank the anonymous referee for their suggestions and Simon
Vaughan for helpful discussion. MJM appreciates support from ERC grant
340442, DJW is supported by ORAU under the NASA Postdoctoral programme
at the NASA Jet Propulsion Laboratory. TPR was funded as part of the
STFC consolidated grant ST/L00075X/1. This work is based on observations
obtained with XMM-Newton, an ESA science mission with instruments and
contributions directly funded by ESA Member States and NASA.
NR 60
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 11
PY 2015
VL 454
IS 3
BP 3134
EP 3142
DI 10.1093/mnras/stv2214
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7QY
UT WOS:000368000400067
ER
PT J
AU Mouginot, J
Rignot, E
Scheuchl, B
Fenty, I
Khazendar, A
Morlighem, M
Buzzi, A
Paden, J
AF Mouginot, J.
Rignot, E.
Scheuchl, B.
Fenty, I.
Khazendar, A.
Morlighem, M.
Buzzi, A.
Paden, J.
TI Fast retreat of Zachariae Isstrom, northeast Greenland
SO SCIENCE
LA English
DT Article
ID ICE-SHEET; CONTINENTAL-SHELF; GLACIER; BENEATH; DYNAMICS; CAVITY; WATER
AB After 8 years of decay of its ice shelf, Zachariae Isstrom, a major glacier of northeast Greenland that holds a 0.5-meter sea-level rise equivalent, entered a phase of accelerated retreat in fall 2012. The acceleration rate of its ice velocity tripled, melting of its residual ice shelf and thinning of its grounded portion doubled, and calving is now occurring at its grounding line. Warmer air and ocean temperatures have caused the glacier to detach from a stabilizing sill and retreat rapidly along a downward-sloping, marine-based bed. Its equal-ice-volume neighbor, Nioghalvfjerdsfjorden, is also melting rapidly but retreating slowly along an upward-sloping bed. The destabilization of this marine-based sector will increase sea-level rise from the Greenland Ice Sheet for decades to come.
C1 [Mouginot, J.; Rignot, E.; Scheuchl, B.; Morlighem, M.; Buzzi, A.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, E.; Fenty, I.; Khazendar, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Paden, J.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
RP Mouginot, J (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM jmougino@uci.edu
RI Morlighem, Mathieu/O-9942-2014; Rignot, Eric/A-4560-2014
OI Morlighem, Mathieu/0000-0001-5219-1310; Rignot, Eric/0000-0002-3366-0481
FU NASA [NNX13AI84A, NNX14AB93G, NNX13AD53A, NNX15AD55G]; NSF [ANT-0424589]
FX This work was performed under NASA grants NNX13AI84A (E.R.), NNX14AB93G
(E.R.), NNX13AD53A (J.P.), and NNX15AD55G (M.M.), and NSF grant
ANT-0424589 (J.P.). The work of I.F., A.K., and E.R. was carried at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. We gratefully acknowledge European Space Agency,
Canadian Space Agency, Japan Aerospace Exploration Agency, Agenzia
Spaziale Italiana, National Aeronautics and Space Administration, and
Deutsches Zentrum fur Luft- und Raumfahrt e.V. for providing SAR data
and Polar Space Task Group for coordination of SAR acquisitions.
NR 25
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U1 11
U2 40
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 DEC 11
PY 2015
VL 350
IS 6266
BP 1357
EP 1361
DI 10.1126/science.aac7111
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CY1JL
UT WOS:000366162400038
PM 26563135
ER
PT J
AU Aird, J
Alexander, DM
Ballantyne, DR
Civano, F
Del-Moro, A
Hickox, RC
Lansbury, GB
Mullaney, JR
Bauer, FE
Brandt, WN
Comastri, A
Fabian, AC
Gandhi, P
Harrison, FA
Luo, B
Stern, D
Treister, E
Zappacosta, L
Ajello, M
Assef, R
Balokovic, M
Boggs, SE
Brightman, M
Christensen, FE
Craig, WW
Elvis, M
Forster, K
Grefenstette, BW
Hailey, CJ
Koss, M
LaMassa, SM
Madsen, KK
Puccetti, S
Saez, C
Urry, CM
Wik, DR
Zhang, W
AF Aird, J.
Alexander, D. M.
Ballantyne, D. R.
Civano, F.
Del-Moro, A.
Hickox, R. C.
Lansbury, G. B.
Mullaney, J. R.
Bauer, F. E.
Brandt, W. N.
Comastri, A.
Fabian, A. C.
Gandhi, P.
Harrison, F. A.
Luo, B.
Stern, D.
Treister, E.
Zappacosta, L.
Ajello, M.
Assef, R.
Balokovic, M.
Boggs, S. E.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Elvis, M.
Forster, K.
Grefenstette, B. W.
Hailey, C. J.
Koss, M.
LaMassa, S. M.
Madsen, K. K.
Puccetti, S.
Saez, C.
Urry, C. M.
Wik, D. R.
Zhang, W.
TI THE NuSTAR EXTRAGALACTIC SURVEY: FIRST DIRECT MEASUREMENTS OF THE
greater than or similar to 10 keV X-RAY LUMINOSITY FUNCTION FOR ACTIVE
GALACTIC NUCLEI AT z > 0.1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; X-rays: galaxies
ID DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; COMPTON-THICK AGN;
POINT-SOURCE CATALOGS; SWIFT-BAT SURVEY; XMM-NEWTON; SEYFERT-GALAXIES;
NUMBER COUNTS; SKY SURVEY; PHOTOMETRIC REDSHIFTS
AB We present the first direct measurements of the rest-frame 10-40 keV X-ray luminosity function (XLF) of active galactic nuclei (AGNs) based on a sample of 94 sources at 0.1 < z < 3, selected at 8-24 keV energies from sources in the Nuclear Spectroscopic Telescope Array (NuSTAR) extragalactic survey program. Our results are consistent with the strong evolution of the AGN population seen in prior, lower-energy studies of the XLF. However, different models of the intrinsic distribution of absorption, which are used to correct for selection biases, give significantly different predictions for the total number of sources in our sample, leading to small, systematic differences in our binned estimates of the XLF. Adopting a model with a lower intrinsic fraction of Compton-thick sources and a larger population of sources with column densities N-H similar to 10(23-24) cm(-2) or a model with stronger Compton reflection component (with a relative normalization of R similar to 2 at all luminosities) can bring extrapolations of the XLF from 2-10 keV into agreement with our NuSTAR sample. Ultimately, X-ray spectral analysis of the NuSTAR sources is required to break this degeneracy between the distribution of absorbing column densities and the strength of the Compton reflection component and thus refine our measurements of the XLF. Furthermore, the models that successfully describe the high-redshift population seen by NuSTAR tend to over-predict previous, high-energy measurements of the local XLF, indicating that there is evolution of the AGN population that is not fully captured by the current models.
C1 [Aird, J.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Aird, J.; Alexander, D. M.; Del-Moro, A.; Lansbury, G. B.; Gandhi, P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Civano, F.; LaMassa, S. M.; Urry, C. M.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Comastri, A.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Harrison, F. A.; Brightman, M.; Forster, K.; Grefenstette, B. W.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Zappacosta, L.; Puccetti, S.] INAF, Osservatorio Astron Roma, I-00040 Rome, Italy.
[Ajello, M.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Assef, R.] Univ Diego Portales, Nucleo Astron Fac Ingn, Santiago, Chile.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
[Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wik, D. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wik, D. R.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Zhang, W.] West Virginia Wesleyan Coll, Phys & Engn Dept, Buckhannon, WV 26201 USA.
RP Aird, J (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM jaird@ast.cam.ac.uk
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU National Aeronautics and Space Administration; ERC Advanced Grant
FEEDBACK at the University of Cambridge; Institute of Advanced Study,
Durham University; Science and Technology Facilities Council (STFC)
[ST/I001573/1, ST/K501979/1, ST/J003697/1]; Leverhulme Trust; Caltech
Kingsley Visitor Program; NSF [AST 1008067]; NASA [11-ADAP11-0218,
GO3-14150C]; Alfred P. Sloan Research Fellowship; Dartmouth Class of
Faculty Fellowship; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT
[1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy,
Development, and Tourisms Millennium Science Initiative [IC120009]; NASA
NuSTAR [44A-1092750]; NASA ADP grant [NNX10AC99G]; ASI/INAF
[I/037/12/0011/13]; NASA Earth and Space Science Fellowship Program
[NNX14AQ07H]
FX This work 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). We
acknowledge financial support from: ERC Advanced Grant FEEDBACK at the
University of Cambridge (J.A., A.C.F.); a COFUND Junior Research
Fellowship from the Institute of Advanced Study, Durham University
(J.A.); the Science and Technology Facilities Council (STFC) grants
ST/I001573/1 (D.M.A. and A.D.M.), ST/K501979/1 (G.B.L.), and
ST/J003697/1 (P.G.); the Leverhulme Trust (D.M.A.); the Caltech Kingsley
Visitor Program (D.M.A., A.C.); NSF award AST 1008067 (D.R.B.); NASA
grants 11-ADAP11-0218 and GO3-14150C (F.C.); an Alfred P. Sloan Research
Fellowship and a Dartmouth Class of 1962 Faculty Fellowship (R.C.H.);
CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., E.T.); FONDECYT
1141218 (F.E.B.) and 1120061 (E.T.); "EMBIGGEN" Anillo ACT1101 (F.E.B.,
E.T.); the Ministry of Economy, Development, and Tourisms Millennium
Science Initiative through grant IC120009, awarded to The Millennium
Institute of Astrophysics, MAS (F.E.B.); NASA NuSTAR subcontract
44A-1092750 and NASA ADP grant NNX10AC99G (W.N.B., B.L.); ASI/INAF grant
I/037/12/0011/13 (A.C., L.Z.); and NASA Earth and Space Science
Fellowship Program grant NNX14AQ07H (M.B.).
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 DEC 10
PY 2015
VL 815
IS 1
AR 66
DI 10.1088/0004-637X/815/1/66
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000066
ER
PT J
AU Annuar, A
Gandhi, P
Alexander, DM
Lansbury, GB
Arevalo, P
Ballantyne, DR
Balokovic, M
Bauer, FE
Boggs, SE
Brandt, WN
Brightman, M
Christensen, FE
Craig, WW
Del Moro, A
Hailey, CJ
Harrison, FA
Hickox, RC
Matt, G
Puccetti, S
Ricci, C
Rigby, JR
Stern, D
Walton, DJ
Zappacosta, L
Zhang, W
AF Annuar, A.
Gandhi, P.
Alexander, D. M.
Lansbury, G. B.
Arevalo, P.
Ballantyne, D. R.
Balokovic, M.
Bauer, F. E.
Boggs, S. E.
Brandt, W. N.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Del Moro, A.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
Matt, G.
Puccetti, S.
Ricci, C.
Rigby, J. R.
Stern, D.
Walton, D. J.
Zappacosta, L.
Zhang, W.
TI NuSTAR OBSERVATIONS OF THE COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND
ULTRALUMINOUS X-RAY SOURCE CANDIDATE IN NGC 5643
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; techniques: spectroscopic; X-rays:
galaxies; X-rays: individual (NGC 5643, NGC 5643 X-1)
ID SEYFERT 2 GALAXIES; HOLMBERG IX X-1; XMM-NEWTON; BLACK-HOLES; NEARBY
GALAXIES; CIRCINUS GALAXY; EMISSION-LINE; BROAD-BAND; SPECTRAL MODELS;
COMPLETE CENSUS
AB We present two Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the local Seyfert 2 active galactic nucleus (AGN) and an ultraluminous X-ray source (ULX) candidate in NGC 5643. Together with archival data from Chandra, XMM-Newton, and Swift-BAT, we perform a high-quality broadband spectral analysis of the AGN over two decades in energy (similar to 0.5-100 keV). Previous X-ray observations suggested that the AGN is obscured by a Compton-thick (CT) column of obscuring gas along our line of sight. However, the lack of high-quality greater than or similar to 10 keV observations, together with the presence of a nearby X-ray luminous source, NGC 5643 X-1, have left significant uncertainties in the characterization of the nuclear spectrum. NuSTAR now enables the AGN and NGC 5643 X-1 to be separately resolved above 10 keV for the first time and allows a direct measurement of the absorbing column density toward the nucleus. The new data show that the nucleus is indeed obscured by a CT column of N-H greater than or similar to 5 x 10(24) cm(-2). The range of 2-10 keV absorption-corrected luminosity inferred from the bestfitting models is L-2-10,L-int = (0.8-1.7) x 10(42) erg s(-1), consistent with that predicted from multiwavelength intrinsic luminosity indicators. In addition, we also study the NuSTAR data for NGC 5643 X-1 and show that it exhibits evidence of a spectral cutoff at energy E similar to 10 keV, similar to that seen in other ULXs observed by NuSTAR. Along with the evidence for significant X-ray luminosity variations in the 3-8 keV band from 2003 to 2014, our results further strengthen the ULX classification of NGC 5643 X-1.
C1 [Annuar, A.; Gandhi, P.; Alexander, D. M.; Lansbury, G. B.; Del Moro, A.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Gandhi, P.] Univ Southampton, Fac Phys Sci & Engn, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Arevalo, P.; Bauer, F. E.] EMBIGGEN Anillo, Concepcion, Chile.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Balokovic, M.; Brightman, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Millenium Inst Astrophys, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 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.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Puccetti, S.; Zappacosta, L.] INAF, Osservatorio Astron Roma, I-00040 Rome, Italy.
[Ricci, C.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Rigby, J. R.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Annuar, A (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Ballantyne,
David/0000-0001-8128-6976; Lansbury, George/0000-0002-5328-9827
FU Majlis Amanah Rakyat (MARA) Malaysia; Science and Technology Facilities
Council (STFC) [ST/J003697/1, ST/I0015731/1, ST/K501979/1]; Leverhulme
Trust; NASA Headquarters under the NASA Earth and Space Science
Fellowship Program [NNX14AQ07H]; CONICYT-Chile grants Basal-CATA
[PFB-06/2007]; FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101]; Ministry
of Economy, Development, and Tourism's Millennium Science Initiative
[IC120009]; National Aeronautics and Space Administration (NASA)
FX The authors thank the anonymous referee for useful comments that have
helped to improve the paper. We thank Chris Done for some discussions on
the residuals around the iron line complex. A.A. thanks Wasutep Luangtip
for useful discussion on NGC 5643 X-1 and help with the MARX simulation.
We also thank Neil Gehrels and the Swift team for the simultaneous
Swift-XRT observation. We acknowledge financial support from Majlis
Amanah Rakyat (MARA) Malaysia (A. A.), the Science and Technology
Facilities Council (STFC) grants ST/J003697/1 (P.G.), ST/I0015731/1
(D.M.A. and A.D.M.), and ST/K501979/1 (G.B.L.), the Leverhulme Trust
(D.M.A.), NASA Headquarters under the NASA Earth and Space Science
Fellowship Program grant NNX14AQ07H (M.B.), CONICYT-Chile grants
Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT 1141218 (F.E.B.), and
"EMBIGGEN" Anillo ACT1101 (F.E.B.); the Ministry of Economy,
Development, and Tourism's Millennium Science Initiative through grant
IC120009, awarded to The Millennium Institute of Astrophysics, MAS
(F.E.B.).; NuSTAR is a project led by the California Institute of
Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL),
and funded by the National Aeronautics and Space Administration (NASA).
We thank the NuSTAR Operations, Software and Calibrations teams for
support with 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), and the XRT Data Analysis Software (XRT-DAS). This
research also made use of the data obtained through the High Energy
Astrophysics Science Archive Research Center (HEASARC) Online Service,
provided by the NASA/Goddard Space Flight Center, and the NASA/IPAC
extragalactic Database (NED) operated by JPL, Caltech under contract
with NASA.
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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 DEC 10
PY 2015
VL 815
IS 1
AR 36
DI 10.1088/0004-637X/815/1/36
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000036
ER
PT J
AU Dobbs-Dixon, I
Agol, E
Deming, D
AF Dobbs-Dixon, Ian
Agol, Eric
Deming, Drake
TI SPECTRAL ECLIPSE TIMING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; methods: observational; planets and satellites:
atmospheres; planets and satellites: individual (HD 209458b)
ID EXOPLANET HD 189733B; UPSILON ANDROMEDAE B; EXTRASOLAR PLANET; HOT
JUPITERS; PHASE CURVES; EMISSION-SPECTRUM; LIGHT CURVES; ATMOSPHERE;
209458B; MAP
AB We utilize multi-dimensional simulations of varying equatorial jet strength to predict wavelength-dependent variations in the eclipse times of gas-giant planets. A displaced hot spot introduces an asymmetry in the secondary eclipse light curve that manifests itself as a measured offset in the timing of the center of eclipse. A multi-wavelength observation of secondary eclipse, one probing the timing of barycentric eclipse at short wavelengths and another probing at longer wavelengths, will reveal the longitudinal displacement of the hot spot and break the degeneracy between this effect and that associated with the asymmetry due to an eccentric orbit. The effect of time offsets was first explored in the IRAC wavebands by Williams et al. Here we improve upon their methodology, extend to a broad range of wavelengths, and demonstrate our technique on a series of multi-dimensional radiative-hydrodynamical simulations of HD 209458b with varying equatorial jet strength and hot-spot displacement. Simulations with the largest hot-spot displacement result in timing offsets of up to 100 s in the infrared. Though we utilize a particular radiative hydrodynamical model to demonstrate this effect, the technique is model independent. This technique should allow a much larger survey of hot-spot displacements with the James Webb Space Telescope than currently accessible with time-intensive phase curves, hopefully shedding light on the physical mechanisms associated with thermal energy advection in irradiated gas giants.
C1 [Dobbs-Dixon, Ian] NYU, Dept Phys, Abu Dhabi, U Arab Emirates.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Agol, Eric; Deming, Drake] NASA, Astrobiol Inst, Virtual Planet Lab, Washington, DC USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Dobbs-Dixon, I (reprint author), NYU, Dept Phys, POB 129188, Abu Dhabi, U Arab Emirates.
OI /0000-0002-0802-9145; Dobbs-Dixon, Ian/0000-0002-4989-6501
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH05ZDA001C]; NASA through Space Telescope
Science Institute [12181]; NASA [NAS 5-26555]; NSF CAREER Grant
[AST-0645416]
FX We thank Nick Cowan for valuable discussions and Adam Burrows for
providing opacities. This work was partly performed as part of the NASA
Astrobiology Institute's Virtual Planetary Laboratory Lead Team,
supported by the National Aeronautics and Space Administration through
the NASA Astrobiology Institute under Cooperative Agreement solicitation
NNH05ZDA001C. Additional support for this work was provided by NASA
through grant number 12181 from the Space Telescope Science Institute,
which is operated by AURA, Inc., under NASA contract NAS 5-26555. We
would also like to acknowledge the use of NASA's High End Computing
Program computer systems. Additional support for this work was provided
by NASA through an award issued by JPL/Caltech. We acknowledge support
from NSF CAREER Grant AST-0645416.
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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 DEC 10
PY 2015
VL 815
IS 1
AR 60
DI 10.1088/0004-637X/815/1/60
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000060
ER
PT J
AU Kallman, T
Dorodnitsyn, A
Blondin, J
AF Kallman, T.
Dorodnitsyn, A.
Blondin, J.
TI X-RAY POLARIZATION FROM HIGH-MASS X-RAY BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; radiative transfer; scattering; X-rays: binaries
ID LIGHT-SOURCE ANISOTROPY; THIN STELLAR ENVELOPES; NEUTRON-STAR;
SCATTERING POLARIZATION; THOMSON SCATTERING; COMPTON-SCATTERING; VELA
X-1; WIND; ACCRETION; EMISSION
AB X-ray astronomy allows study of objects that may be associated with compact objects, i.e., neutron stars or black holes, and also may contain strong magnetic fields. Such objects are categorically nonspherical, and likely noncircular when projected on the sky. Polarization allows study of such geometric effects, and X-ray polarimetry is likely to become feasible for a significant number of sources in the future. Potential targets for future X-ray polarization observations are the high-mass X-ray binaries (HMXBs), which consist of a compact object in orbit with an early-type star. In this paper we show that X-ray polarization from HMXBs has a distinct signature that depends on the source inclination and orbital phase. The presence of the X-ray source displaced from the star creates linear polarization even if the primary wind is spherically symmetric whenever the system is viewed away from conjunction. Direct X-rays dilute this polarization whenever the X-ray source is not eclipsed; at mid-eclipse the net polarization is expected to be small or zero if the wind is circularly symmetric around the line of centers. Resonance line scattering increases the scattering fraction, often by large factors, over the energy band spanned by resonance lines. Real winds are not expected to be spherically symmetric, or circularly symmetric around the line of centers, owing to the combined effects of the compact object gravity and ionization on the wind hydrodynamics. A sample calculation shows that this creates polarization fractions ranging up to tens of percent at mid-eclipse.
C1 [Kallman, T.] NASA GSFC, Greenbelt, MD 20771 USA.
[Dorodnitsyn, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dorodnitsyn, A.] Space Res Inst, Moscow 117997, Russia.
[Blondin, J.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
RP Kallman, T (reprint author), NASA GSFC, Code 662, Greenbelt, MD 20771 USA.
OI Blondin, John/0000-0001-9691-6803
FU NASA astrophysics theory program [10-ATP10-0171]
FX Support was provided through grant 10-ATP10-0171 through the NASA
astrophysics theory program.
NR 48
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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 DEC 10
PY 2015
VL 815
IS 1
AR 53
DI 10.1088/0004-637X/815/1/53
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000053
ER
PT J
AU Kane, SR
Barclay, T
Hartmann, M
Hatzes, AP
Jensen, ELN
Ciardi, DR
Huber, D
Wright, JT
Quintana, EV
AF Kane, Stephen R.
Barclay, Thomas
Hartmann, Michael
Hatzes, Artie P.
Jensen, Eric L. N.
Ciardi, David R.
Huber, Daniel
Wright, Jason T.
Quintana, Elisa V.
TI ON THE STELLAR COMPANION TO THE EXOPLANET HOSTING STAR 30 ARIETIS B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (30 Ari B); techniques: high
angular resolution; techniques: photometric; techniques: radial
velocities
ID SOLAR-TYPE STARS; RADIAL-VELOCITY; SPECTROSCOPIC BINARIES; PLANETARY
ORBITS; ADAPTIVE OPTICS; MULTIPLICITY; SYSTEMS; STABILITY; III.;
VALIDATION
AB A crucial aspect of understanding planet formation is determining the binarity of the host stars. Results from radial velocity (RV) surveys and the follow-up of Kepler exoplanet candidates have demonstrated that stellar binarity certainly does not exclude the presence of planets in stable orbits and the configuration may in fact be relatively common. Here we present new results for the 30 Arietis system which confirms that the B component hosts both planetary and stellar companions. Keck AO imaging provides direct detection of the stellar companion and additional RV data are consistent with an orbiting star. We present a revised orbit of the known planet along with photometry during predicted transit times. Finally, we provide constraints on the properties of the stellar companion based on orbital stability considerations.
C1 [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Barclay, Thomas; Quintana, Elisa V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Hartmann, Michael; Hatzes, Artie P.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA.
[Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
[Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM skane@sfsu.edu
OI Jensen, Eric/0000-0002-4625-7333; Wright, Jason/0000-0001-6160-5888;
Ciardi, David/0000-0002-5741-3047
FU Australian Research Council [DE140101364]; NASA [NNX14AB92G]; NASA
Senior Fellowship at the Ames Research Center; NASA Keck PI Data Award;
W. M. Keck Foundation
FX The authors would like to thank Elliott Horch, Steve Howell, and Suvrath
Mahadevan for several useful discussions. Thanks are also due to the
anonymous referee whose helpful comments improved the manuscript. D.H.
acknowledges support by the Australian Research Council's Discovery
Projects funding scheme (project number DE140101364) and by NASA under
Grant NNX14AB92G issued through the Kepler Participating Scientist
Program. E.V.Q. is supported by a NASA Senior Fellowship at the Ames
Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA. This work made use of the Digitized Sky
Survey (DSS) hosted by the Mikulski Archive for Space Telescopes (MAST).
This work was supported by a NASA Keck PI Data Award, administered by
the NASA Exoplanet Science Institute. Data presented herein were
obtained at the W. M. Keck Observatory from telescope time allocated to
the National Aeronautics and Space Administration through the agencys
scientific partnership with the California Institute of Technology and
the University of California. 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. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 36
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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 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2015
VL 815
IS 1
AR 32
DI 10.1088/0004-637X/815/1/32
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000032
ER
PT J
AU Marcu-Cheatham, DM
Pottschmidt, K
Kuhnel, M
Muller, S
Falkner, S
Caballero, I
Finger, MH
Jenke, PJ
Wilson-Hodge, CA
Furst, F
Grinberg, V
Hemphill, PB
Kreykenbohm, I
Klochkov, D
Rothschild, RE
Terada, Y
Enoto, T
Iwakiri, W
Wolff, MT
Becker, PA
Wood, KS
Wilms, J
AF Marcu-Cheatham, Diana M.
Pottschmidt, Katja
Kuehnel, Matthias
Mueller, Sebastian
Falkner, Sebastian
Caballero, Isabel
Finger, Mark H.
Jenke, Peter J.
Wilson-Hodge, Colleen A.
Fuerst, Felix
Grinberg, Victoria
Hemphill, Paul B.
Kreykenbohm, Ingo
Klochkov, Dmitry
Rothschild, Richard E.
Terada, Yukikatsu
Enoto, Teruaki
Iwakiri, Wataru
Wolff, Michael T.
Becker, Peter A.
Wood, Kent S.
Wilms, Joern
TI THE TRANSIENT ACCRETING X-RAY PULSAR XTE J1946+274: STABILITY OF X-RAY
PROPERTIES AT LOW FLUX AND UPDATED ORBITAL SOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; pulsars: individual (XTE J1946+274); X-rays:
binaries
ID CYCLOTRON LINE ENERGY; NEUTRON-STARS; GX 304-1; OUTBURST; BINARY;
LUMINOSITY; DISCOVERY; A0535+26; ABSORPTION; MODELS
AB We present a timing and spectral analysis of the X-ray pulsar XTE J1946+274 observed with Suzaku during an outburst decline in 2010 October and compare with previous results. XTE J1946+274 is a transient X-ray binary consisting of a Be-type star and a neutron star with a 15.75 s pulse period in a 172 days orbit with 2-3 outbursts per orbit during phases of activity. We improve the orbital solution using data from multiple instruments. The X-ray spectrum can be described by an absorbed Fermi-Dirac cut-off power-law model along with a narrow Fe K alpha line at 6.4 keV and a weak Cyclotron Resonance Scattering Feature (CRSF) at similar to 35 keV. The Suzaku data are consistent with the previously observed continuum flux versus iron line flux correlation expected from fluorescence emission along the line of sight. However, the observed iron line flux is slightly higher, indicating the possibility of a higher iron abundance or the presence of non-uniform material. We argue that the source most likely has only been observed in the subcritical (non-radiation dominated) state since its pulse profile is stable over all observed luminosities and the energy of the CRSF is approximately the same at the highest (similar to 5 x 10(37) erg s(-1)) and lowest (similar to 5. x 10(36) erg s(-1)) observed 3-60 keV luminosities.
C1 [Marcu-Cheatham, Diana M.; Pottschmidt, Katja] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Marcu-Cheatham, Diana M.; Pottschmidt, Katja] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Marcu-Cheatham, Diana M.; Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kuehnel, Matthias; Mueller, Sebastian; Falkner, Sebastian; Kreykenbohm, Ingo; Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Bamberg, Germany.
[Kuehnel, Matthias; Mueller, Sebastian; Falkner, Sebastian; Kreykenbohm, Ingo; Wilms, Joern] Univ Erlangen Nurnberg, ECAP, Bamberg, Germany.
[Caballero, Isabel] Univ Paris Diderot, CNRS INSU, Lab AIM, CEA DSM IRFU SAp,CEA IRFU, F-91191 Gif Sur Yvette, France.
[Finger, Mark H.] Univ Space Res Assoc, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Jenke, Peter J.] Univ Alabama, Huntsville, AL 35899 USA.
[Wilson-Hodge, Colleen A.] NASA, Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[Fuerst, Felix] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Grinberg, Victoria] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Hemphill, Paul B.; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Klochkov, Dmitry] Univ Tubingen IAAT, Inst Astron & Astrophys, Tubingen, Germany.
[Terada, Yukikatsu] Saitama Univ, Grad Sch Sci & Engn, Sakura Ku, Saitama, Saitama 3388570, Japan.
[Enoto, Teruaki] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Enoto, Teruaki] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068502, Japan.
[Iwakiri, Wataru] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan.
[Wolff, Michael T.; Wood, Kent S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Becker, Peter A.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
RP Marcu-Cheatham, DM (reprint author), Univ Maryland Baltimore Cty, CRESST, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Falkner,
Sebastian/0000-0001-5209-991X; Hemphill, Paul/0000-0002-1676-6954
FU Suzaku NASA Guest Observer grant [NNX11AD41G]; NASA Astrophysical Data
Analysis Program grant [12-ADAP12-0118]; Bundesministerium fur
Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und
Raumfahrt [50OR1113, 50OR1207]; Deutsche Forschungsgemeinschaft [WI
1860/11-1]; NASA through the Smithsonian Astrophysical Observatory (SAO)
[SV3-73016]; Chandra X-Ray Center (CXC) and Science Instruments; NASA
[NAS8-03060]
FX D.M.M.-C. and K.P. acknowledge support by Suzaku NASA Guest Observer
grant NNX11AD41G and NASA Astrophysical Data Analysis Program grant
12-ADAP12-0118. We acknowledge funding by the Bundesministerium fur
Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und
Raumfahrt grants 50OR1113 and 50OR1207 and Deutsche
Forschungsgemeinschaft grant WI 1860/11-1. We thank John E. Davis for
the development of the SLXfig module, which was used to create Figure 4.
M.T.W. and K.S.W. acknowledge support by the Chief of Naval Research and
NASA Astrophysical Data Analysis Program grant 12-ADAP12-0118. V.G.
acknowledges support 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.
NR 57
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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 DEC 10
PY 2015
VL 815
IS 1
AR 44
DI 10.1088/0004-637X/815/1/44
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000044
ER
PT J
AU Nesvold, ER
Kuchner, MJ
AF Nesvold, Erika R.
Kuchner, Marc J.
TI A SMACK MODEL OF COLLIDING PLANETESIMALS IN THE beta PICTORIS DEBRIS
DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; circumstellar matter; methods: numerical;
planet-disk interactions; planets and satellites: individual (beta
Pictoris)
ID PLANET-FINDING CAMPAIGN; DIRECTLY IMAGED PLANET; EDGEWORTH-KUIPER BELT;
DUST DISK; COLLISIONAL EVOLUTION; CIRCUMSTELLAR DISKS; AU MICROSCOPII;
GIANT PLANETS; SUPER-EARTHS; INNER DISK
AB We present a new model of the beta Pictoris disk-and-planet system that simulates both the planetesimal collisions and the dynamics of the resulting dust grains, allowing us to model features and asymmetries in both thermal and scattered light images of the disk. Our two-part model first simulates the collisional and dynamical evolution of the planetesimals with the Superparticle-Method Algorithm for Collisions in Kuiper belts and then simulates the dynamical evolution of the resulting dust grains with a standard Bulirsch-Stoer N-body integrator. Given the observed inclination and eccentricity of the beta Pictoris b planet, the model neatly ties together several features of the disk: the central hole in the submillimeter images, the two-disk "x"-pattern seen in scattered light, and possibly even the clumpy gas seen by ALMA. We also find that most of the dust in the beta Pictoris system is likely produced outside the ring at 60-100 AU. Instead of a birth ring, this disk has a "stirring ring" at 60-100 AU where the high-velocity collisions produced by the secular wave launched by the planet are concentrated. The two-disk x-pattern arises because collisions occur more frequently at the peaks and troughs of the secular wave. The perturbations of the disk in this region create an azimuthally and vertically asymmetric spatial distribution of collisions, which could yield an azimuthal clump of gas without invoking resonances or an additional planet.
C1 [Nesvold, Erika R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Nesvold, Erika R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 21230 USA.
RP Nesvold, ER (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM enesvold@carnegiescience.edu; Marc.Kuchner@nasa.gov
OI Nesvold, Erika/0000-0002-7484-5124
FU NASA Planetary Geology and Geophysics grant [PGG11-0032]; ALMA Student
Observing Support Program through NRAO; NASA Astrobiology Institute
through the Goddard Center for Astrobiology
FX Erika Nesvold and Marc Kuchner are supported in part by NASA Planetary
Geology and Geophysics grant PGG11-0032. Erika Nesvold is supported in
part by the ALMA Student Observing Support Program through NRAO. Marc
Kuchner is supported in part by the NASA Astrobiology Institute through
the Goddard Center for Astrobiology.
NR 70
TC 9
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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 DEC 10
PY 2015
VL 815
IS 1
AR 61
DI 10.1088/0004-637X/815/1/61
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000061
ER
PT J
AU Rivers, E
Balokovic, M
Arevalo, P
Bauer, FE
Boggs, SE
Brandt, WN
Brightman, M
Christensen, FE
Craig, WW
Gandhi, P
Hailey, CJ
Harrison, F
Koss, M
Ricci, C
Stern, D
Walton, DJ
Zhang, WW
AF Rivers, E.
Balokovic, M.
Arevalo, P.
Bauer, F. E.
Boggs, S. E.
Brandt, W. N.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Hailey, C. J.
Harrison, F.
Koss, M.
Ricci, C.
Stern, D.
Walton, D. J.
Zhang, W. W.
TI THE NuSTAR VIEW OF REFLECTION AND ABSORPTION IN NGC 7582
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 7582); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY TELESCOPE; TIMING-EXPLORER; SPECTRAL
SURVEY; GALAXIES; NGC-7582; TORUS
AB NGC 7582 is a well-studied X-ray bright Seyfert 2 with moderately heavy (N-H similar to 10(23)-10(24) cm(-2)), highly variable absorption and strong reflection spectral features. The spectral shape changed around the year 2000, dropping in observed flux and becoming much more highly absorbed. Two scenarios have been put forth to explain this spectral change: (1) the central X-ray source partially "shut off" around this time, decreasing in intrinsic luminosity, with a delayed decrease in reflection features due to the light-crossing time of the Compton-thick material or (2) the source became more heavily obscured, with only a portion of the power law continuum leaking through. NuSTAR observed NGC 7582 twice in 2012, two weeks apart, in order to quantify the reflection using high-quality data above 10 keV. We find that the most plausible scenario is that NGC 7582 has recently become more heavily absorbed by a patchy torus with a covering fraction of similar to 80%-90% and an equatorial column density of similar to 3 x 10(24) cm(-2). We find the need for an additional highly variable full-covering absorber with N-H = (4-6) x 10(23) cm(-2) in the line of sight, possibly associated with a hidden broad line region.
C1 [Rivers, E.; Balokovic, M.; Brightman, M.; Harrison, F.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 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, Davey Lab 104, Dept Phys, University Pk, PA 16802 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rivers, E (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM erivers@caltech.edu
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C, 44A-1092750]; National Aeronautics and Space
Administration; NASA/GSFC; NASA/IPAC Extragalactic Database; NASA
Headquarters [NNX14AQ07H]; Fondecyt grant [1140304]; CONICYT-Chile
[Basal-CATA PFB-06/2007, FONDECYT 1141218, Anillo ACT1101]; Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
[IC120009]; Swiss National Science Foundation; Ambizione fellowship
[PZ00P2 154799/1]
FX We would like to thank the anonymous referee for helpful and
constructive comments contributing to this work. This work was supported
under NASA Contract No. NNG08FD60C and sub-contract No. 44A-1092750. We
have 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). This work has
made use of also made use of RXTE and Swift archival data and HEASARC
online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic
Database, operated by JPL/California Institute of Technology under
contract with NASA. M.B. acknowledges support from NASA Headquarters
under the NASA Earth and Space Science Fellowship Program, grant
NNX14AQ07H. P.A. acknowledges financial support form Fondecyt grant
1140304. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA
PFB-06/2007, FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and the
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative through grant IC120009, awarded to The Millennium Institute
of Astrophysics, MAS. M.K. acknowledges support from the Swiss National
Science Foundation and Ambizione fellowship grant PZ00P2 154799/1.
NR 35
TC 8
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U1 0
U2 7
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 DEC 10
PY 2015
VL 815
IS 1
AR 55
DI 10.1088/0004-637X/815/1/55
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000055
ER
PT J
AU Schuler, SC
Vaz, ZA
Santrich, OJK
Cunha, K
Smith, VV
King, JR
Teske, JK
Ghezzi, L
Howell, SB
Isaacson, H
AF Schuler, Simon C.
Vaz, Zachary A.
Santrich, Orlando J. Katime
Cunha, Katia
Smith, Verne V.
King, Jeremy R.
Teske, Johanna K.
Ghezzi, Luan
Howell, Steve B.
Isaacson, Howard
TI DETAILED ABUNDANCES OF STARS WITH SMALL PLANETS DISCOVERED BY KEPLER. I.
THE FIRST SAMPLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; planets and satellites: terrestrial
planets; stars: abundances; stars: atmospheres
ID SOLAR-TYPE STARS; GALACTIC CHEMICAL EVOLUTION; CANDIDATE HOST STARS;
MAIN-SEQUENCE STARS; OPEN CLUSTER DWARFS; RED-GIANT STARS;
LINE-DATA-BASE; SUN-LIKE STARS; 4 EARTH RADII; LITHIUM ABUNDANCES
AB We present newly derived stellar parameters and the detailed abundances of 19 elements of seven stars with small planets discovered by NASA's Kepler Mission. Each star, save one, has at least one planet with a radius <= 1.6 R-circle plus, suggesting a primarily rocky composition. The stellar parameters and abundances are derived from high signal-to-noise ratio, high-resolution echelle spectroscopy obtained with the 10 m Keck I telescope and High Resolution Echelle Spectrometer using standard spectroscopic techniques. The metallicities of the seven stars range from -0.32 to + 0.13 dex, with an average metallicity that is subsolar, supporting previous suggestions that, unlike Jupiter-type giant planets, small planets do not form preferentially around metal-rich stars. The abundances of elements other than iron are in line with a population of Galactic disk stars, and despite our modest sample size, we find hints that the compositions of stars with small planets are similar to stars without known planets and with Neptune-size planets, but not to those of stars with giant planets. This suggests that the formation of small planets does not require exceptional host-star compositions and that small planets may be ubiquitous in the Galaxy. We compare our derived abundances (which have typical uncertainties of less than or similar to 0.04 dex) to the condensation temperature of the elements; a correlation between the two has been suggested as a possible signature of rocky planet formation. None of the stars demonstrate the putative rocky planet signature, despite at least three of the stars having rocky planets estimated to contain enough refractory material to produce the signature, if real. More detailed abundance analyses of stars known to host small planets are needed to verify our results and place ever more stringent constraints on planet formation models.
C1 [Schuler, Simon C.; Vaz, Zachary A.] Univ Tampa, Tampa, FL 33606 USA.
[Santrich, Orlando J. Katime; Cunha, Katia; Smith, Verne V.] Observ Nacl, Rio De Janeiro, RJ, Brazil.
[Cunha, Katia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[King, Jeremy R.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Teske, Johanna K.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ghezzi, Luan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Schuler, SC (reprint author), Univ Tampa, Tampa, FL 33606 USA.
EM sschuler@ut.edu; zachary.vaz@spartans.ut.edu; osantrich@on.br;
kcunha@noao.edu; vsmith@noao.edu; jking2@clemson.edu;
jteske@carnegiescience.edu; lghezzi@cfa.harvard.edu;
steve.b.howell@nasa.gov; hisaacson@berkeley.edu
OI Schuler, Simon/0000-0001-7203-8014; Isaacson, Howard/0000-0002-0531-1073
FU National Aeronautics and Space Administration as part of the Kepler
Participating Scientist Program [NNX12AD19G]; W. M. Keck Foundation
FX We graciously thank F. Valdes at NOAO for his help with the processing
of the Keck/HIRES data, as well as G. Marcy and A. Howard for their role
in obtaining the KFOP/Keck spectra. S. C. S. acknowledges support
provided by grant NNX12AD19G from the National Aeronautics and Space
Administration as part of the Kepler Participating Scientist Program.
Some data presented herein were obtained at the W. M. Keck Observatory
from telescope time allocated to the National Aeronautics and Space
Administration through the agency's scientific partnership with the
California Institute of Technology and the University of California. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. Additional data were obtained at Kitt Peak
National Observatory, National Optical Astronomy Observatory, which is
operated by the Association of Universities for Research in Astronomy
(AURA) under cooperative agreement with the National Science Foundation.
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.
NR 131
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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 DEC 10
PY 2015
VL 815
IS 1
AR 5
DI 10.1088/0004-637X/815/1/5
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000005
ER
PT J
AU Sekanina, Z
Kracht, R
AF Sekanina, Zdenek
Kracht, Rainer
TI WAS COMET C/1945 X1 (DU TOIT) A DWARF, SOHO-LIKE KREUTZ SUNGRAZER?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; methods: data analysis
ID ORBITAL EVOLUTION; SOLAR; SYSTEM; SUN; FRAGMENTATION; HIERARCHY; ORIGIN;
BIRTH
AB The goal of this investigation is to reinterpret and upgrade the astrometric and other data on comet C/1945 X1, the least prominent among the Kreutz system sungrazers discovered from the ground in the twentieth century. The central issue is to appraise the pros and cons of a possibility that this object is-despite its brightness reported at discovery-a dwarf Kreutz sungrazer. We confirm Marsden's conclusion that C/1945 X1 has a common parent with C/1882 R1 and C/1965 S1, in line with the Sekanina & Chodas scenario of their origin in the framework of the Kreutz system's evolution. We integrate the orbit of C/1882 R1 back to the early twelfth century and then forward to around 1945 to determine the nominal direction of the line of apsides and perform a Fourier analysis to get insight into effects of the indirect planetary perturbations. To better understand the nature of C/1945 X1, its orbital motion, fate, and role in the hierarchy of the Kreutz system, as well as to attempt detecting the comet's possible terminal outburst shortly after perihelion and answer the question in the title of this investigation, we closely examined the relevant Boyden Observatory logbooks and identified both the photographs with the comet's known images and nearly 20 additional patrol plates, taken both before and after perihelion, on which the comet or traces of its debris will be searched for, once the process of their digitization, currently conducted as part of the Harvard College Observatory's DASCH Project, has been completed and the scanned copies made available to the scientific community.
C1 [Sekanina, Zdenek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sekanina, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Zdenek.Sekanina@jpl.nasa.gov; R.Kracht@t-online.de
NR 38
TC 0
Z9 0
U1 5
U2 5
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 DEC 10
PY 2015
VL 815
IS 1
AR 52
DI 10.1088/0004-637X/815/1/52
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000052
ER
PT J
AU Switzer, ER
Chang, TC
Masui, KW
Pen, UL
Voytek, TC
AF Switzer, E. R.
Chang, T. -C.
Masui, K. W.
Pen, U. -L.
Voytek, T. C.
TI INTERPRETING THE UNRESOLVED INTENSITY OF COSMOLOGICALLY REDSHIFTED LINE
RADIATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE diffuse radiation; large-scale structure of universe; methods: data
analysis; methods: statistical
ID LARGE-SCALE STRUCTURE; DARK ENERGY SURVEY; POWER SPECTRUM; ERROR BARS;
DATA SETS; TO 0.8; REIONIZATION; TOMOGRAPHY; EPOCH; ANISOTROPY
AB Intensity mapping experiments survey the spectrum of diffuse line radiation rather than detect individual objects at high signal-to-noise ratio. Spectral maps of unresolved atomic and molecular line radiation contain three-dimensional information about the density and environments of emitting gas. and efficiently probe cosmological volumes out to high redshift. Intensity mapping survey volumes also contain all other sources of radiation at the frequencies of interest. Continuum foregrounds are typically similar to 10(2)-10(3) times brighter than the cosmological signal. The instrumental response to bright foregrounds will produce new spectral degrees of freedom that are not known in advance, nor necessarily spectrally smooth. The intrinsic spectra of foregrounds may also not be well. known in advance. We describe a general class of quadratic estimators to analyze data from single-dish intensity mapping experiments. and determine contaminated spectral modes from the data themselves. The key attribute of foregrounds is not that they are spectrally smooth, but instead that they have fewer bright spectral degrees of freedom than the cosmological signal. Spurious correlations between the signal and foregrounds produce additional bias. Compensation for signal attenuation must estimate and correct this bias. A successful intensity mapping experiment will control instrumental systematics that spread variance into new modes, and it must observe a large enough volume that contaminant modes can be determined independently from the signal on scales of interest.
C1 [Switzer, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chang, T. -C.] Acad Sinica, Inst Astron & Astrophys, AS NTU, Taipei 10617, Taiwan.
[Masui, K. W.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Masui, K. W.; Pen, U. -L.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada.
[Pen, U. -L.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Voytek, T. C.] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA.
[Voytek, T. C.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
RP Switzer, ER (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM eric.r.switzer@nasa.gov
FU Canada Foundation for Innovation
FX E.S. acknowledges support as a CITA fellow, where much of this work was
conducted. We thank John Ford, Anish Roshi, and the rest of the GBT
staff for their support, especially in understanding instrument
response. Computations were performed on the GPC supercomputer at the
SciNet HPC Consortium. SciNet is funded by the Canada Foundation for
Innovation.
NR 77
TC 4
Z9 4
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 DEC 10
PY 2015
VL 815
IS 1
AR 51
DI 10.1088/0004-637X/815/1/51
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000051
ER
PT J
AU Vivian, U
Hemmati, S
Darvish, B
Mobasher, B
Nayyeri, H
Dickinson, M
Stern, D
Spinrad, H
Mallery, R
AF Vivian, U.
Hemmati, Shoubaneh
Darvish, Behnam
Mobasher, Bahram
Nayyeri, Hooshang
Dickinson, Mark
Stern, Daniel
Spinrad, Hyron
Mallery, Ryan
TI A CORRELATION BETWEEN Ly alpha SPECTRAL LINE PROFILE AND REST-FRAME UV
MORPHOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM
ID LYMAN BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES;
EXTRAGALACTIC LEGACY SURVEY; ORIGINS DEEP SURVEY; GOODS-SOUTH FIELD;
ULTRAVIOLET-SPECTRA; KECK SPECTROSCOPY; NEBULAR EMISSION; TO 2-3
AB We explore the relationship between the spectral shape of the Ly alpha emission and the UV morphology of the host galaxy using a sample of 304 Ly alpha-emitting BVi-dropouts at 3 < z < 7 in the Great Observatories Origins Deep Survey and Cosmic Evolution Survey fields. Using our extensive reservoir of high-quality Keck DEIMOS spectra combined with Hubble Space Telescope WFC3 data, we measure the Ly alpha line asymmetries for individual galaxies and compare them to axial ratios measured from observed J-and H-band (restframe UV) images. We find that the Ly alpha skewness exhibits a large scatter at small elongation (a/b < 2), and this scatter decreases as the axial ratio increases. Comparison of this trend to radiative transfer models and various results from the literature suggests that these high-redshift Ly alpha emitters are not likely to be intrinsically round and symmetric disks, but they probably host galactic outflows traced by Ly alpha emitting clouds. The ionizing sources are centrally located, and the optical depth is a good indicator of the absorption and scattering events on the escape path of Ly alpha photons from the source. Our results find no evidence of evolution in Ly alpha asymmetry or axial ratio with look-back time.
C1 [Vivian, U.; Hemmati, Shoubaneh; Darvish, Behnam; Mobasher, Bahram; Nayyeri, Hooshang; Mallery, Ryan] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Nayyeri, Hooshang] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Mallery, Ryan] Rebell Photon, Houston, TX 77021 USA.
RP Vivian, U (reprint author), Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA.
EM vivianu@ucr.edu
FU Thirty Meter Telescope International Observatory; UC Chancellor's
Postdoctoral Fellowship Program; W. M. Keck Foundation
FX We thank the referee for a thorough review and many helpful suggestions
that improved the paper. V.U. acknowledges helpful discussions of the
various statistical tests with C.W.K. Chiang, as well as partial funding
support from the Thirty Meter Telescope International Observatory and
the UC Chancellor's Postdoctoral Fellowship Program. The work of D. S.
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. 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 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. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 57
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 DEC 10
PY 2015
VL 815
IS 1
AR 57
DI 10.1088/0004-637X/815/1/57
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ4XB
UT WOS:000367105000057
ER
PT J
AU Barnes, RA
Brown, SW
Lykke, KR
Guenther, B
Butler, JJ
Schwarting, T
Turpie, K
Moyer, D
Deluccia, F
Moeller, C
AF Barnes, Robert A.
Brown, Steven W.
Lykke, Keith R.
Guenther, Bruce
Butler, James J.
Schwarting, Thomas
Turpie, Kevin
Moyer, David
Deluccia, Frank
Moeller, Christopher
TI Comparison of two methodologies for calibrating satellite instruments in
the visible and near-infrared
SO APPLIED OPTICS
LA English
DT Article
ID SPECTRAL IRRADIANCE; RADIANCE RESPONSIVITY; SEAWIFS
AB Traditionally, satellite instruments that measure Earth-reflected solar radiation in the visible and near infrared wavelength regions have been calibrated for radiance responsivity in a two-step method. In the first step, the relative spectral response (RSR) of the instrument is determined using a nearly monochromatic light source such as a lamp-illuminated monochromator. These sources do not typically fill the field of view of the instrument nor act as calibrated sources of light. Consequently, they only provide a relative (not absolute) spectral response for the instrument. In the second step, the instrument views a calibrated source of broadband light, such as a lamp-illuminated integrating sphere. The RSR and the sphere's absolute spectral radiance are combined to determine the absolute spectral radiance responsivity (ASR) of the instrument. More recently, a full-aperture absolute calibration approach using widely tunable monochromatic lasers has been developed. Using these sources, the ASR of an instrument can be determined in a single step on a wavelength-by-wavelength basis. From these monochromatic ASRs, the responses of the instrument bands to broadband radiance sources can be calculated directly, eliminating the need for calibrated broadband light sources such as lamp-illuminated integrating spheres. In this work, the traditional broadband source-based calibration of the Suomi National Preparatory Project Visible Infrared Imaging Radiometer Suite sensor is compared with the laser-based calibration of the sensor. Finally, the impact of the new full-aperture laser-based calibration approach on the on-orbit performance of the sensor is considered.
C1 [Barnes, Robert A.] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
[Brown, Steven W.; Lykke, Keith R.] NIST, Gaithersburg, MD 20899 USA.
[Guenther, Bruce] Stellar Solut Inc, Chantilly, VA 20151 USA.
[Butler, James J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schwarting, Thomas] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Turpie, Kevin] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Moyer, David; Deluccia, Frank] Aerosp Corp, El Segundo, CA 90245 USA.
[Moeller, Christopher] Univ Wisconsin, Madison, WI 53706 USA.
RP Brown, SW (reprint author), NIST, Gaithersburg, MD 20899 USA.
EM swbrown@nist.gov
FU Intramural NIST DOC [9999-NIST]
NR 27
TC 2
Z9 2
U1 0
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 DEC 10
PY 2015
VL 54
IS 35
BP 10376
EP 10396
DI 10.1364/AO.54.010376
PG 21
WC Optics
SC Optics
GA CY7RH
UT WOS:000366605900013
PM 26836861
ER
PT J
AU Nathues, A
Hoffmann, M
Schaefer, M
Le Corre, L
Reddy, V
Platz, T
Cloutis, EA
Christensen, U
Kneissl, T
Li, JY
Mengel, K
Schmedemann, N
Schaefer, T
Russell, CT
Applin, DM
Buczkowski, DL
Izawa, MRM
Keller, HU
O'Brien, DP
Pieters, CM
Raymond, CA
Ripken, J
Schenk, PM
Schmidt, BE
Sierks, H
Sykes, MV
Thangjam, GS
Vincent, JB
AF Nathues, A.
Hoffmann, M.
Schaefer, M.
Le Corre, L.
Reddy, V.
Platz, T.
Cloutis, E. A.
Christensen, U.
Kneissl, T.
Li, J. -Y.
Mengel, K.
Schmedemann, N.
Schaefer, T.
Russell, C. T.
Applin, D. M.
Buczkowski, D. L.
Izawa, M. R. M.
Keller, H. U.
O'Brien, D. P.
Pieters, C. M.
Raymond, C. A.
Ripken, J.
Schenk, P. M.
Schmidt, B. E.
Sierks, H.
Sykes, M. V.
Thangjam, G. S.
Vincent, J. -B.
TI Sublimation in bright spots on (1) Ceres
SO NATURE
LA English
DT Article
ID WATER-VAPOR; ASTEROIDS; VESTA; MARS; CONDENSATION; EVOLUTION; MINERALS;
PLUME; DAWN
AB The dwarf planet (1) Ceres, the largest object in the main asteroid belt(1) with a mean diameter of about 950 kilometres, is located at a mean distance from the Sun of about 2.8 astronomical units (one astronomical unit is the Earth-Sun distance). Thermal evolution models suggest that it is a differentiated body with potential geological activity(2,3). Unlike on the icy satellites of Jupiter and Saturn, where tidal forces are responsible for spewing briny water into space, no tidal forces are acting on Ceres. In the absence of such forces, most objects in the main asteroid belt are expected to be geologically inert. The recent discovery(4) of water vapour absorption near Ceres and previous detection of bound water and OH near and on Ceres (refs 5-7) have raised interest in the possible presence of surface ice. Here we report the presence of localized bright areas on Ceres from an orbiting imager(8). These unusual areas are consistent with hydrated magnesium sulfates mixed with dark background material, although other compositions are possible. Of particular interest is a bright pit on the floor of crater Occator that exhibits probable sublimation of water ice, producing haze clouds inside the crater that appear and disappear with a diurnal rhythm. Slow-moving condensed-ice or dust particles(9,10) may explain this haze. We conclude that Ceres must have accreted material from beyond the 'snow line' 11, which is the distance from the Sun at which water molecules condense.
C1 [Nathues, A.; Hoffmann, M.; Schaefer, M.; Le Corre, L.; Reddy, V.; Platz, T.; Christensen, U.; Schaefer, T.; Ripken, J.; Sierks, H.; Thangjam, G. S.; Vincent, J. -B.] Max Planck Inst Solar Syst Res, Gottingen, Germany.
[Le Corre, L.; Reddy, V.; Li, J. -Y.; O'Brien, D. P.; Sykes, M. V.] Planetary Sci Inst, Tucson, AZ USA.
[Cloutis, E. A.; Applin, D. M.; Izawa, M. R. M.] Univ Winnipeg, Winnipeg, MB R3B 2E9, Canada.
[Kneissl, T.; Schmedemann, N.] Free Univ Berlin, Berlin, Germany.
[Mengel, K.] Tech Univ Clausthal, D-38678 Clausthal Zellerfeld, Germany.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Buczkowski, D. L.] Johns Hopkins Univ, Laurel, MD USA.
[Izawa, M. R. M.] Royal Ontario Museum, Toronto, ON M5S 2C6, Canada.
[Keller, H. U.] TU Braunschweig, Braunschweig, Germany.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Schenk, P. M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Schmidt, B. E.] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Nathues, A (reprint author), Max Planck Inst Solar Syst Res, Gottingen, Germany.
EM Nathues@mps.mpg.de
RI Platz, Thomas/F-7539-2013;
OI Platz, Thomas/0000-0002-1253-2034; Schmidt, Britney/0000-0001-7376-8510;
Le Corre, Lucille/0000-0003-0349-7932
FU Max Planck Society; German Space Agency, DLR
FX We thank the Dawn operations team for the development, cruise, orbital
insertion and operations of the Dawn spacecraft at Ceres. We also thank
the FC operations team, especially P. G. Gutierrez-Marques, I. Hall and
I. Buttner. The FC project is financially supported by the Max Planck
Society and the German Space Agency, DLR.
NR 34
TC 24
Z9 25
U1 6
U2 17
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 DEC 10
PY 2015
VL 528
IS 7581
BP 237
EP +
DI 10.1038/nature15754
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CX9VH
UT WOS:000366053300035
PM 26659183
ER
PT J
AU De Sanctis, MC
Ammannito, E
Raponi, A
Marchi, S
McCord, TB
McSween, HY
Capaccioni, F
Capria, MT
Carrozzo, FG
Ciarniello, M
Longobardo, A
Tosi, F
Fonte, S
Formisano, M
Frigeri, A
Giardino, M
Magni, G
Palomba, E
Turrini, D
Zambon, F
Combe, JP
Feldman, W
Jaumann, R
McFadden, LA
Pieters, CM
Prettyman, T
Toplis, M
Raymond, CA
Russell, CT
AF De Sanctis, M. C.
Ammannito, E.
Raponi, A.
Marchi, S.
McCord, T. B.
McSween, H. Y.
Capaccioni, F.
Capria, M. T.
Carrozzo, F. G.
Ciarniello, M.
Longobardo, A.
Tosi, F.
Fonte, S.
Formisano, M.
Frigeri, A.
Giardino, M.
Magni, G.
Palomba, E.
Turrini, D.
Zambon, F.
Combe, J. -P.
Feldman, W.
Jaumann, R.
McFadden, L. A.
Pieters, C. M.
Prettyman, T.
Toplis, M.
Raymond, C. A.
Russell, C. T.
TI Ammoniated phyllosilicates with a likely outer Solar System origin on
(1) Ceres
SO NATURE
LA English
DT Article
ID SURFACE-COMPOSITION; OPTICAL-CONSTANTS; CLAY-MINERALS; MU-M;
PROTOPLANETARY DISCS; SPECTRAL VARIABILITY; CRYSTALLINE H2O-ICE;
SPECTROSCOPY; REFLECTANCE; ASTEROIDS
AB Studies of the dwarf planet (1) Ceres using ground-based and orbiting telescopes have concluded that its closest meteoritic analogues are the volatile-rich CI and CM carbonaceous chondrites(1,2). Water in clay minerals(3), ammoniated phyllosilicates(4), or a mixture of Mg(OH)(2) (brucite), Mg2CO3 and iron-rich serpentine(5,6) have all been proposed to exist on the surface. In particular, brucite has been suggested from analysis of the mid-infrared spectrum of Ceres(6). But the lack of spectral data across telluric absorption bands in the wavelength region 2.5 to 2.9 micrometres-where the OH stretching vibration and the H2O bending overtone are found-has precluded definitive identifications. In addition, water vapour around Ceres has recently been reported(7), possibly originating from localized sources. Here we report spectra of Ceres from 0.4 to 5 micrometres acquired at distances from similar to 82,000 to 4,300 kilometres from the surface. Our measurements indicate widespread ammoniated phyllosilicates across the surface, but no detectable water ice. Ammonia, accreted either as organic matter or as ice, may have reacted with phyllosilicates on Ceres during differentiation. This suggests that material from the outer Solar System was incorporated into Ceres, either during its formation at great heliocentric distance or by incorporation of material transported into the main asteroid belt.
C1 [De Sanctis, M. C.; Ammannito, E.; Raponi, A.; Marchi, S.; Capaccioni, F.; Capria, M. T.; Carrozzo, F. G.; Ciarniello, M.; Longobardo, A.; Tosi, F.; Fonte, S.; Formisano, M.; Frigeri, A.; Giardino, M.; Magni, G.; Palomba, E.; Turrini, D.; Zambon, F.] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Marchi, S.] SW Res Inst, Boulder, CO 80302 USA.
[McCord, T. B.; Combe, J. -P.] Bear Fight Inst, Winthrop, WA 98862 USA.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Feldman, W.; Prettyman, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Jaumann, R.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Toplis, M.] Univ Toulouse 3, Observ Midi Pyrenees, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP De Sanctis, MC (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM mariacristina.desanctis@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Zambon, Francesca/0000-0002-4190-6592; Frigeri,
Alessandro/0000-0002-9140-3977; Carrozzo, Filippo
Giacomo/0000-0002-0391-6407; McFadden, Lucy/0000-0002-0537-9975;
Prettyman, Thomas/0000-0003-0072-2831; Turrini,
Diego/0000-0002-1923-7740; Palomba, Ernesto/0000-0002-9101-6774; Tosi,
Federico/0000-0003-4002-2434
FU Italian Space Agency (ASI); National Aeronautic and Space Administration
(NASA, USA); Deutsches Zentrum fur Luft- und Raumfahrt (DLR, Germany);
Italian Space Agency
FX We thank the following institutions and agencies, which supported this
work: the Italian Space Agency (ASI), the National Aeronautic and Space
Administration (NASA, USA) and the Deutsches Zentrum fur Luft- und
Raumfahrt (DLR, Germany). The VIR was funded and coordinated by the
Italian Space Agency and built by SELEX ES, with the scientific
leadership of the Institute for Space Astrophysics and Planetology,
Italian National Institute for Astrophysics, Italy, and is operated by
the Institute for Space Astrophysics and Planetology, Rome, Italy. A
portion of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract to NASA. We thank J.
L. Bishop and D. Takir for reviews, and D. Takir for providing spectra
of carbonaceous chondrites plotted in Fig. 2.
NR 43
TC 30
Z9 30
U1 7
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 DEC 10
PY 2015
VL 528
IS 7581
BP 241
EP +
DI 10.1038/nature16172
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CX9VH
UT WOS:000366053300036
PM 26659184
ER
PT J
AU Xu, JT
Lin, Y
Connell, JW
Dai, LM
AF Xu, Jiantie
Lin, Yi
Connell, John W.
Dai, Liming
TI Nitrogen-Doped Holey Graphene as an Anode for Lithium-Ion Batteries with
High Volumetric Energy Density and Long Cycle Life
SO SMALL
LA English
DT Article
ID ACTIVE ELECTRODE MATERIAL; RATE CAPABILITY; ELECTROCHEMICAL PROPERTIES;
PERFORMANCE; STORAGE; FABRICATION; CAPACITY; NANOSHEETS; METAL;
ULTRACAPACITORS
C1 [Xu, Jiantie; Dai, Liming] Case Western Reserve Univ, Dept Macromol Sci & Engn, Cleveland, OH 44106 USA.
[Lin, Yi] NIA, Hampton, VA 23666 USA.
[Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
[Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Lin, Y (reprint author), NIA, 100 Exploration Way, Hampton, VA 23666 USA.
EM yi.lin@nianet.org; john.w.connell@nasa.gov; liming.dai@case.edu
FU AFOSR [FA9550-12-1-0037]; NSF [CMMI-1400274, DMR-1106160]; Internal
Research and Development (IRAD) program at NASA Langley Research Center;
Leading Edge Aeronautics Research for NASA (LEARN) program [NNX13AB88A]
FX The authors are grateful for financial support from AFOSR
(FA9550-12-1-0037), NSF (CMMI-1400274, DMR-1106160). Y.L. and J.W.C.
acknowledge the financial support from the Internal Research and
Development (IRAD) program at NASA Langley Research Center. Y.L. is also
grateful for the support from the Leading Edge Aeronautics Research for
NASA (LEARN) program (Grant number NNX13AB88A).
NR 45
TC 15
Z9 16
U1 34
U2 148
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1613-6810
EI 1613-6829
J9 SMALL
JI Small
PD DEC 9
PY 2015
VL 11
IS 46
BP 6179
EP 6185
DI 10.1002/smll.201501848
PG 7
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA CX9WP
UT WOS:000366056900005
PM 26485602
ER
PT J
AU Weinmaier, T
Probst, AJ
La Duc, MT
Ciobanu, D
Cheng, JF
Ivanova, N
Rattei, T
Vaishampayan, P
AF Weinmaier, Thomas
Probst, Alexander J.
La Duc, Myron T.
Ciobanu, Doina
Cheng, Jan-Fang
Ivanova, Natalia
Rattei, Thomas
Vaishampayan, Parag
TI A viability-linked metagenomic analysis of cleanroom environments:
eukarya, prokaryotes, and viruses
SO MICROBIOME
LA English
DT Article
DE Indoor microbiome; PMA; Viability; Comparative metagenomics; Spacecraft;
Cleanroom; Viruses; Bacteria; Fungi
ID PROPIDIUM MONOAZIDE; BACTERIAL COMMUNITIES; SEQUENCING DATA; WATER
SAMPLES; SEARCH TOOL; SPACECRAFT; DIVERSITY; ROOMS; PCR; DISTINGUISH
AB Background: Recent studies posit a reciprocal dependency between the microbiomes associated with humans and indoor environments. However, none of these metagenome surveys has considered the viability of constituent microorganisms when inferring impact on human health.
Results: Reported here are the results of a viability-linked metagenomics assay, which (1) unveil a remarkably complex community profile for bacteria, fungi, and viruses and (2) bolster the detection of underrepresented taxa by eliminating biases resulting from extraneous DNA. This approach enabled, for the first time ever, the elucidation of viral genomes from a cleanroom environment. Upon comparing the viable biomes and distribution of phylotypes within a cleanroom and adjoining (uncontrolled) gowning enclosure, the rigorous cleaning and stringent control countermeasures of the former were observed to select for a greater presence of anaerobes and spore-forming microflora. Sequence abundance and correlation analyses suggest that the viable indoor microbiome is influenced by both the human microbiome and the surrounding ecosystem(s).
Conclusions: The findings of this investigation constitute the literature's first ever account of the indoor metagenome derived from DNA originating solely from the potential viable microbial population. Results presented in this study should prove valuable to the conceptualization and experimental design of future studies on indoor microbiomes aimed at inferring impact on human health.
C1 [Weinmaier, Thomas; Rattei, Thomas] Univ Vienna, Dept Microbiol & Ecosyst Sci, Div Computat Syst Biol, Vienna, Austria.
[Probst, Alexander J.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[La Duc, Myron T.; Vaishampayan, Parag] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
[La Duc, Myron T.] Precis Sci, Scottsdale, AZ USA.
[Ciobanu, Doina; Cheng, Jan-Fang; Ivanova, Natalia] DOE Joint Genome Inst, Walnut Creek, CA USA.
RP Vaishampayan, P (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
EM vaishamp@jpl.nasa.gov
RI Rattei, Thomas/F-1366-2011; Probst, Alexander/K-2813-2016;
OI Rattei, Thomas/0000-0002-0592-7791; Weinmaier,
Thomas/0000-0002-9552-3220; Ivanova, Natalia/0000-0002-5802-9485
FU NASA
FX Part of the research described in this study was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research was funded by NASA Research Announcement (NRA) ROSES 2011
awarded to PV and NI.
NR 55
TC 6
Z9 7
U1 7
U2 19
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 2049-2618
J9 MICROBIOME
JI Microbiome
PD DEC 8
PY 2015
VL 3
AR 62
DI 10.1186/s40168-015-0129-y
PG 14
WC Microbiology
SC Microbiology
GA CY4BW
UT WOS:000366354600001
PM 26642878
ER
PT J
AU Ade, PAR
Arnold, K
Atlas, M
Baccigalupi, C
Barron, D
Boettger, D
Borrill, J
Chapman, S
Chinone, Y
Cukierman, A
Dobbs, M
Ducout, A
Dunner, R
Elleflot, T
Errard, J
Fabbian, G
Feeney, S
Feng, C
Gilbert, A
Goeckner-Wald, N
Groh, J
Hall, G
Halverson, NW
Hasegawa, M
Hattori, K
Hazumi, M
Hill, C
Holzapfel, WL
Hori, Y
Howe, L
Inoue, Y
Jaehnig, GC
Jaffe, AH
Jeong, O
Katayama, N
Kaufman, JP
Keating, B
Kermish, Z
Keskitalo, R
Kisner, T
Kusaka, A
Le Jeune, M
Lee, AT
Leitch, EM
Leon, D
Li, Y
Linder, E
Lowry, L
Matsuda, F
Matsumura, T
Miller, N
Montgomery, J
Myers, MJ
Navaroli, M
Nishino, H
Okamura, T
Paar, H
Peloton, J
Pogosian, L
Poletti, D
Puglisi, G
Raum, C
Rebeiz, G
Reichardt, CL
Richards, PL
Ross, C
Rotermund, KM
Schenck, DE
Sherwin, BD
Shimon, M
Shirley, I
Siritanasak, P
Smecher, G
Stebor, N
Steinbach, B
Suzuki, A
Suzuki, J
Tajima, O
Takakura, S
Tikhomirov, A
Tomaru, T
Whitehorn, N
Wilson, B
Yadav, A
Zahn, A
Zahn, O
AF Ade, Peter A. R.
Arnold, Kam
Atlas, Matt
Baccigalupi, Carlo
Barron, Darcy
Boettger, David
Borrill, Julian
Chapman, Scott
Chinone, Yuji
Cukierman, Ari
Dobbs, Matt
Ducout, Anne
Dunner, Rolando
Elleflot, Tucker
Errard, Josquin
Fabbian, Giulio
Feeney, Stephen
Feng, Chang
Gilbert, Adam
Goeckner-Wald, Neil
Groh, John
Hall, Grantland
Halverson, Nils W.
Hasegawa, Masaya
Hattori, Kaori
Hazumi, Masashi
Hill, Charles
Holzapfel, William L.
Hori, Yasuto
Howe, Logan
Inoue, Yuki
Jaehnig, Gregory C.
Jaffe, Andrew H.
Jeong, Oliver
Katayama, Nobuhiko
Kaufman, Jonathan P.
Keating, Brian
Kermish, Zigmund
Keskitalo, Reijo
Kisner, Theodore
Kusaka, Akito
Le Jeune, Maude
Lee, Adrian T.
Leitch, Erik M.
Leon, David
Li, Yun
Linder, Eric
Lowry, Lindsay
Matsuda, Frederick
Matsumura, Tomotake
Miller, Nathan
Montgomery, Josh
Myers, Michael J.
Navaroli, Martin
Nishino, Haruki
Okamura, Takahiro
Paar, Hans
Peloton, Julien
Pogosian, Levon
Poletti, Davide
Puglisi, Giuseppe
Raum, Christopher
Rebeiz, Gabriel
Reichardt, Christian L.
Richards, Paul L.
Ross, Colin
Rotermund, Kaja M.
Schenck, David E.
Sherwin, Blake D.
Shimon, Meir
Shirley, Ian
Siritanasak, Praween
Smecher, Graeme
Stebor, Nathan
Steinbach, Bryan
Suzuki, Aritoki
Suzuki, Jun-ichi
Tajima, Osamu
Takakura, Satoru
Tikhomirov, Alexei
Tomaru, Takayuki
Whitehorn, Nathan
Wilson, Brandon
Yadav, Amit
Zahn, Alex
Zahn, Oliver
TI POLARBEAR constraints on cosmic birefringence and primordial magnetic
fields
SO PHYSICAL REVIEW D
LA English
DT Article
ID MICROWAVE BACKGROUND POLARIZATION; LARGE-SCALE STRUCTURE; B-MODE
POLARIZATION; 100 SQUARE DEGREES; FARADAY-ROTATION; GRAVITY-WAVES; TEV
BLAZARS; SPTPOL DATA; ANISOTROPIES; SIGNATURE
AB We constrain anisotropic cosmic birefringence using four-point correlations of even-parity E-mode and odd-parity B-mode polarization in the cosmic microwave background measurements made by the POLARization of the Background Radiation (POLARBEAR) experiment in its first season of observations. We find that the anisotropic cosmic birefringence signal from any parity-violating processes is consistent with zero. The Faraday rotation from anisotropic cosmic birefringence can be compared with the equivalent quantity generated by primordial magnetic fields if they existed. The POLARBEAR non-detection translates into a 95% confidence level (C.L.) upper limit of 93 nanogauss (nG) on the amplitude of an equivalent primordial magnetic field inclusive of systematic uncertainties. This four-point correlation constraint on Faraday rotation is about 15 times tighter than the upper limit of 1380 nG inferred from constraining the contribution of Faraday rotation to two-point correlations of B-modes measured by Planck in 2015. Metric perturbations sourced by primordial magnetic fields would also contribute to the B-mode power spectrum. Using the POLARBEAR measurements of the B-mode power spectrum (two-point correlation), we set a 95% C.L. upper limit of 3.9 nG on primordial magnetic fields assuming a flat prior on the field amplitude. This limit is comparable to what was found in the Planck 2015 two-point correlation analysis with both temperature and polarization. We perform a set of systematic error tests and find no evidence for contamination. This work marks the first time that anisotropic cosmic birefringence or primordial magnetic fields have been constrained from the ground at subdegree scales.
C1 [Ade, Peter A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales.
[Arnold, Kam; Atlas, Matt; Elleflot, Tucker] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Baccigalupi, Carlo; Fabbian, Giulio; Puglisi, Giuseppe] SISSA, I-34136 Trieste, Italy.
[Barron, Darcy; Chinone, Yuji; Cukierman, Ari; Goeckner-Wald, Neil; Groh, John; Hall, Grantland; Hill, Charles; Holzapfel, William L.; Hori, Yasuto; Jeong, Oliver; Lee, Adrian T.; Myers, Michael J.; Raum, Christopher; Richards, Paul L.; Sherwin, Blake D.; Shirley, Ian; Steinbach, Bryan; Whitehorn, Nathan; Zahn, Oliver] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Boettger, David; Dunner, Rolando] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile.
[Borrill, Julian; Errard, Josquin; Keskitalo, Reijo; Kisner, Theodore] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Borrill, Julian; Errard, Josquin; Keskitalo, Reijo; Kisner, Theodore] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chapman, Scott; Ross, Colin; Rotermund, Kaja M.; Tikhomirov, Alexei] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Dobbs, Matt; Gilbert, Adam; Montgomery, Josh; Smecher, Graeme] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada.
[Ducout, Anne; Feeney, Stephen; Jaffe, Andrew H.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Dept Phys, London SW7 2AZ, England.
[Feng, Chang] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Halverson, Nils W.; Jaehnig, Gregory C.; Schenck, David E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Halverson, Nils W.; Schenck, David E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, Nils W.; Jaehnig, Gregory C.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hasegawa, Masaya; Hattori, Kaori; Hazumi, Masashi; Inoue, Yuki; Nishino, Haruki; Okamura, Takahiro; Suzuki, Jun-ichi; Tajima, Osamu; Takakura, Satoru; Tomaru, Takayuki] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Hasegawa, Masaya; Hazumi, Masashi; Inoue, Yuki; Tajima, Osamu] SOKENDAI Grad Univ Adv Studies, Miura, Kanagawa 2400115, Japan.
[Hazumi, Masashi; Katayama, Nobuhiko] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Kermish, Zigmund] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Kusaka, Akito; Lee, Adrian T.; Linder, Eric] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Le Jeune, Maude; Peloton, Julien; Poletti, Davide] Univ Paris Diderot, AstroParticule & Cosmol, Ctr Natl Rech Sci,Inst Rech Lois Fondamentales Un, Inst Natl Phys Nucl & Phys Particules,Commissaria, Paris, France.
[Leitch, Erik M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Leitch, Erik M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Li, Yun; Pogosian, Levon] Simon Fraser Univ, Dept Phys, Burnaby, BC V5A 1S6, Canada.
[Matsumura, Tomotake] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Miller, Nathan] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Rebeiz, Gabriel] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA.
[Reichardt, Christian L.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia.
[Sherwin, Blake D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA.
[Shimon, Meir] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Suzuki, Aritoki] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Takakura, Satoru] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
RP Feng, C (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM chang.feng@uci.edu
OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt,
Christian/0000-0003-2226-9169
FU Department of Energy [DE-AC02-05CH11231]; National Science Foundation
[AST-0618398, AST-1212230]; MEXT KAKENHI Grants [21111002, 26220709];
KEK Cryogenics Science Center; JSPS Core-to-Core Program (A. Advanced
Research Networks); Natural Sciences and Engineering Research Council;
Canadian Institute for Advanced Research; NSERC; Comision Nacional de
Investigacion Cientifica y Tecnologica de Chile (CONICYT); Simons
Foundation; NSF [AST-1313319]; Ax Center for Experimental Cosmology;
University of Melbourne; INDARK INFN Network; NSF Astronomy and
Astrophysics Postdoctoral Fellowship [AST-1501422]
FX Calculations were performed on the Gordon supercomputer operated for the
Extreme Science and Engineering Discovery Environment by the San Diego
Supercomputer Center and the Edison supercomputer by the National Energy
Research Scientific Computing, supported by the Department of Energy
under Contract No. DE-AC02-05CH11231. The POLARBEAR project is funded by
the National Science Foundation under Grants No. AST-0618398 and No.
AST-1212230. The KEK authors were supported by MEXT KAKENHI Grants No.
21111002 and No. 26220709, and acknowledge support from KEK Cryogenics
Science Center. This work was supported by the JSPS Core-to-Core Program
(A. Advanced Research Networks). The McGill authors acknowledge funding
from the Natural Sciences and Engineering Research Council and Canadian
Institute for Advanced Research. L. P. and Y. L. are supported by a
Discovery Grant from NSERC. The James Ax Observatory operates in the
Parque Astronomico Atacama in Northern Chile under the auspices of the
Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
(CONICYT). K. A. acknowledges support from the Simons Foundation. C. F.
acknowledges support from NSF Grant No. AST-1313319 and the Ax Center
for Experimental Cosmology. C. R. acknowledges support from the
University of Melbourne. C. B., G. F., and G. P. acknowledge partial
support from the INDARK INFN Network. D. B. is supported by a NSF
Astronomy and Astrophysics Postdoctoral Fellowship under Grant No.
AST-1501422. We are grateful to Marc Kamionkowski and Vera Gluscevic for
the insights and suggestions that helped inspire this work.
NR 79
TC 15
Z9 15
U1 6
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD DEC 8
PY 2015
VL 92
IS 12
AR 123509
DI 10.1103/PhysRevD.92.123509
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CY0LH
UT WOS:000366097100003
ER
PT J
AU Chiow, SW
Williams, J
Yu, N
AF Chiow, Sheng-wey
Williams, Jason
Yu, Nan
TI Laser-ranging long-baseline differential atom interferometers for space
SO PHYSICAL REVIEW A
LA English
DT Article
ID GRAVITY; SENSITIVITY; DELAY
AB High-sensitivity differential atom interferometers (AIs) are promising for precision measurements in science frontiers in space, including gravity-field mapping for Earth science studies and gravitational wave detection. Difficulties associated with implementing long-baseline differential AIs have previously included the need for a high optical power, large differential Doppler shifts, and narrow dynamic range. We propose a configuration of twin AIs connected by a laser-ranging interferometer (LRI-AI) to provide precise information of the displacements between the two AI reference mirrors and also to phase-lock the two independent interferometer lasers over long distances, thereby drastically improving the practical feasibility of long-baseline differential AI measurements. We show that a properly implemented LRI-AI can achieve equivalent functionality to the conventional differential AI measurement configuration.
C1 [Chiow, Sheng-wey; Williams, Jason; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yu, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nan.yu@jpl.nasa.gov
NR 36
TC 2
Z9 2
U1 5
U2 14
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
EI 1094-1622
J9 PHYS REV A
JI Phys. Rev. A
PD DEC 7
PY 2015
VL 92
IS 6
AR 063613
DI 10.1103/PhysRevA.92.063613
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA CY0FU
UT WOS:000366082600013
ER
PT J
AU Jones, CM
Driggers, WB
Castro, JI
de Carvalho, MR
AF Jones, Christian M.
Driggers, William B., III
Castro, Jose I.
de Carvalho, Marcelo R.
TI On the attribution of authorship for several elasmobranch species in
Muller and Henle's Systematische Beschreibung der Plagiostomen
(Chondrichthyes, Elasmobranchii)
SO ZOOTAXA
LA English
DT Editorial Material
C1 [Jones, Christian M.; Driggers, William B., III] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39568 USA.
[Castro, Jose I.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Protected Resources Div, Pascagoula, MS 39568 USA.
[de Carvalho, Marcelo R.] Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05502090 Sao Paulo, SP, Brazil.
RP Jones, CM (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39568 USA.
EM christian.jones@noaa.gov; william.driggers@noaa.gov;
jose.castro@noaa.gov; mrcarvalho@ib.usp.br
NR 12
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 DEC 7
PY 2015
VL 4052
IS 5
BP 569
EP 572
DI 10.11646/zootaxa.4052.5.4
PG 4
WC Zoology
SC Zoology
GA CX7MP
UT WOS:000365886300004
PM 26701453
ER
PT J
AU Menezes, AA
Montague, MG
Cumbers, J
Hogan, JA
Arkin, AP
AF Menezes, Amor A.
Montague, Michael G.
Cumbers, John
Hogan, John A.
Arkin, Adam P.
TI Grand challenges in space synthetic biology
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Review
DE resource utilization; manufacturing; life support; space medicine; space
cybernetics; terraforming
ID NITROGEN REMOVAL; CIRCUIT; CELLS; MARS
AB Space synthetic biology is a branch of biotechnology dedicated to engineering biological systems for space exploration, industry and science. There is significant public and private interest in designing robust and reliable organisms that can assist on long-duration astronaut missions. Recent work has also demonstrated that such synthetic biology is a feasible payload minimization and life support approach as well. This article identifies the challenges and opportunities that lie ahead in the field of space synthetic biology, while highlighting relevant progress. It also outlines anticipated broader benefits from this field, because space engineering advances will drive technological innovation on Earth.
C1 [Menezes, Amor A.; Arkin, Adam P.] Univ Calif Berkeley, Calif Inst Quantitat Biosci, Berkeley, CA 94704 USA.
[Montague, Michael G.] Applicat Vital Knowledge, Frederick, MD 21702 USA.
[Cumbers, John] NASA, Ames Res Ctr, Ames Space Portal, Moffett Field, CA 94035 USA.
[Hogan, John A.] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA.
[Arkin, Adam P.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Arkin, Adam P.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94704 USA.
RP Menezes, AA (reprint author), Univ Calif Berkeley, Calif Inst Quantitat Biosci, 2151 Berkeley Way, Berkeley, CA 94704 USA.
EM amenezes@berkeley.edu; aparkin@lbl.gov
RI Arkin, Adam/A-6751-2008;
OI Arkin, Adam/0000-0002-4999-2931; Menezes, Amor/0000-0003-3923-5766
NR 58
TC 4
Z9 4
U1 26
U2 52
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD DEC 6
PY 2015
VL 12
IS 113
AR 20150803
DI 10.1098/rsif.2015.0803
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA4XV
UT WOS:000367807000009
PM 26631337
ER
PT J
AU Mukhopadhyay, B
Khan, A
Gautam, R
AF Mukhopadhyay, Biswajit
Khan, Asif
Gautam, Ritesh
TI Rising and falling river flows: contrasting signals of climate change
and glacier mass balance from the eastern and western Karakoram
SO HYDROLOGICAL SCIENCES JOURNAL-JOURNAL DES SCIENCES HYDROLOGIQUES
LA English
DT Article
DE Karakoram glaciers; Karakoram anomaly; Upper Indus basin; hydrologic
trend analysis; climate change; glacier mass balance
ID UPPER INDUS BASIN; SIACHEN GLACIER; HIMALAYA; TRENDS; VARIABILITY;
PAKISTAN; REGIME; INDIA; SNOW
AB Field observations and geodetic measurements suggest that in the Karakoram Mountains, glaciers are either stable or have expanded since 1990, in sharp contrast to glacier retreats that are prevalently observed in the Himalayas and adjoining high-altitude terrains of central Asia. Decreased discharge in the rivers originating from this region is cited as a supporting evidence for this somewhat anomalous phenomenon. Here, we show that river discharge during the melting season of the glaciers in the eastern and western Karakoram, respectively, exhibits rising and falling trends. We have implemented a statistical procedure involving non-parametric tests combined with a benchmark smoothing technique that has proven to be a powerful method for separating the stochastic component from the trend component in a time series. Precipitation patterns determined from ERA-40 and GPCP data indicate that summer-monsoonal precipitation has increased over the Karakoram Mountains in recent decades. Increasing flows in June and July in the eastern Karakoram are due to an increase in summer-monsoonal precipitation. The rising trend of August discharge is due to an increase in the loss of glacier storage at an approximate average rate of 0.186-0.217mm d(-1) year(-1) during the period 1973-2010. Moreover, this rate is higher than the rate of increase in monsoonal snowfall during the months of August and September. Therefore, most plausibly, glacier mass balance in the eastern Karakoram is negative. In the western Karakoram, river flows show declining trends for all summer months for the period 1966-2010, corresponding to a rate of increase of glacier storage by approximately 0.552-0.644mm d(-1) year(-1), which is also higher than the rate of increase in summer-monsoonal precipitation. The gain of the cryospheric mass in the western Karakoram is in the form of increased thickness of the glaciers and perennial snowpacks instead of areal expansion. This investigation shows two contrasting patterns of trends of river flows that signify both negative and positive mass balance of the Karakoram glaciers. Trends of river flows are spatially and temporally integrated responses of a watershed to changing climate and thereby are important signals of the conditions of the cryospheric component of a watershed where it is highly significant. However, they cannot unequivocally provide indications of the state and fate of the glaciers in the complex hydrometeorological setting of the Karakoram. Extreme caution and care must be exercised in interpreting trends of river discharge in conjunction with climatic data.
C1 [Mukhopadhyay, Biswajit] Jacobs Engn Grp Inc, Water Resources Grp, Ft Worth, TX 76102 USA.
[Khan, Asif] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England.
[Gautam, Ritesh] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
EM biswajitm2009@sbcglobal.net
NR 43
TC 3
Z9 3
U1 4
U2 13
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0262-6667
EI 2150-3435
J9 HYDROLOG SCI J
JI Hydrol. Sci. J.-J. Sci. Hydrol.
PD DEC 2
PY 2015
VL 60
IS 12
BP 2062
EP 2085
DI 10.1080/02626667.2014.947291
PG 24
WC Water Resources
SC Water Resources
GA CY7LH
UT WOS:000366589400001
ER
PT J
AU Bauschlicher, CW
Monk, JD
Lawson, JW
AF Bauschlicher, Charles W., Jr.
Monk, Joshua D.
Lawson, John W.
TI Failure of single phenolic chains and cross-links: Energetics,
mechanisms, and alternative linker design
SO POLYMER
LA English
DT Article
DE Density functional theory; Strain; Linking groups
ID MOLECULAR-DYNAMICS SIMULATIONS; TOTAL-ENERGY CALCULATIONS; REACTIVE
FORCE-FIELD; WAVE BASIS-SET; REAXFF; APPROXIMATION; EXCHANGE
AB The stretching of a single chain of phenolic polymer is studied using density functional theory (DFT) and the reactive force field (ReaxFF) potential. The most detailed studies are performed at 0 K, which shows the breaking of the C(ring)-CH2 bridge bond can be delayed to longer polymer length by a ring opening mechanism that relieves the strain. Molecular dynamics (MD) simulations, using the DFT approach, show that C-CH2 bridge bond breaking occurs much more frequently than the ring opening. The stretching potentials determined using ReaxFF compare favorably with the DFT results. Using ReaxFF, stretching of cross-linked systems were considered and compared to single chains. The effect of changing the linking group on the bond stretching portion of the potential is found to be relatively small, but the effect on the bond energies can be significant. Published by Elsevier Ltd.
C1 [Bauschlicher, Charles W., Jr.; Monk, Joshua D.; Lawson, John W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov
FU ESM project of the NASA STMD
FX This work was supported by the ESM project of the NASA STMD.
NR 26
TC 2
Z9 2
U1 2
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0032-3861
EI 1873-2291
J9 POLYMER
JI Polymer
PD DEC 2
PY 2015
VL 80
BP 265
EP 274
DI 10.1016/j.polymer.2015.10.050
PG 10
WC Polymer Science
SC Polymer Science
GA CX6LW
UT WOS:000365813500029
ER
PT J
AU Schimel, D
Hibbard, K
Costa, D
Cox, P
van der Leeuw, S
AF Schimel, David
Hibbard, Kathy
Costa, Duarte
Cox, Peter
van der Leeuw, Sander
TI Analysis, Integration and Modeling of the Earth System (AIMES):
Advancing the post-disciplinary understanding of coupled
human-environment dynamics in the Anthropocene
SO ANTHROPOCENE
LA English
DT Article
DE Global Earth System Science; Modeling; Human-environment interactions;
AIMES; Future Earth
ID CARBON-CYCLE; SENSITIVITY; CO2; VARIABILITY; SCENARIOS; TRANSPORT;
FEEDBACK; BP
AB The IGBP Analysis, Integration and Modeling of the Earth System (AIMES) project has developed the notion of Earth System Science (ESS). ESS studies how the planet operates as a coupled system of interacting components, which produce emergent behaviors over and beyond the dynamics of the individual components. Many climate models used in the IPCC's 5th Assessment Report (AR5) include representations of the physical climate system and the biological components of the land and ocean carbon cycle. AIMES and its forerunner Global Analysis and Integration of Models (GAIM) helped lay the groundwork for this advance. Subsequently, AIMES has been instrumental in the evolution of climate models into Earth System Models, promoting dialog between the relevant communities to ensure greater consistency in the IPCC assessment process.
Today, society faces interconnected challenges including climate change, financial crises, food security, governance of pandemics, and energy sufficiency. This requires decision makers to understand systemic risks for which the available tools provide insufficient guidance. AIMES is targeting to improve links of science with stakeholders in society to stimulate appropriate societal responses. Under Future Earth, AIMES prioritizes the understanding and modeling of human-environment interactions in the Anthropocene, focusing on gathering consistent data on biophysics and socioeconomics; lessons that can be learnt from past human-environment interactions; and the modeling of planet Earth as a complex system in which human beings are internal components rather than external actors. Key overarching themes include land-use change and the characterization and forecasting of critical transitions (or "tipping points") in the Earth System. (C) 2016 The Authors. Published by Elsevier Ltd.
C1 [Schimel, David] Jet Prop Lab, Pasadena, CA USA.
[Hibbard, Kathy] NASA Headquarters, Washington, DC USA.
[Costa, Duarte; Cox, Peter] Univ Exeter, Exeter EX4 4QJ, Devon, England.
[van der Leeuw, Sander] Arizona State Univ, Tempe, AZ 85287 USA.
RP van der Leeuw, S (reprint author), Arizona State Univ, Tempe, AZ 85287 USA.
EM vanderle@asu.edu
RI Cox, Peter/B-3299-2012
NR 40
TC 0
Z9 0
U1 6
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 2213-3054
J9 ANTHROPOCENE
JI Anthropocene
PD DEC
PY 2015
VL 12
BP 99
EP 106
DI 10.1016/j.ancene.2016.02.001
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DU0OE
UT WOS:000381903600009
ER
PT J
AU Shah, PN
Vold, H
Hensley, D
Envia, E
Stephens, D
AF Shah, Parthiv N.
Vold, Havard
Hensley, Dan
Envia, Edmane
Stephens, David
TI A High-Resolution Continuous-Scan Acoustic Measurement Method for
Turbofan Engine Applications
SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME
LA English
DT Article
ID ORDER TRACKING; FILTER
AB Detailed mapping of the sound field produced by a modern turbofan engine, with its multitude of overlapping noise sources, often requires a large number of microphones to properly resolve the directivity patterns of the constituent tonal and broadband components. This is especially true at high frequencies where the acoustic wavelength is short, or when shielding, scattering, and reflection of the sound field may be present due to installation effects. This paper presents a novel method for measuring the harmonic and broadband content of complex noncompact noise sources using continuously moving (referred to here as continuous-scan (CS)) microphones in conjunction with a state-of-the-art phase-referencing technique. Because the microphones are moving through the sound field produced by the noise sources, they effectively provide infinite spatial resolution of the sound directivity over the scan path. In this method, harmonic (i.e., shaft-coherent) content at the integer multiples of the instantaneous shaft rotational frequency is first extracted from the time signal using a tachometer signal and the Vold-Kalman (VK) filter. The residual broadband signal is then filtered in the time domain in fractional octave bands. The broadband spectra of the signals from the moving microphones are then computed at arbitrary positions along their scan paths using weighted averages (based on Chebyshev polynomial zero-crossings) and the assumption of a complex envelope that varies slowly over a spatial scale whose lower bound is set by the acoustic wavenumber. A benefit of this method is that the decomposition of the total measured sound field into a stochastic superposition of components preserves a meaningful phase definition for each "partial field" associated with a given shaft order (SO). This preservation of phase data enables the forward or backward projection of each of these partial fields using acoustical holography (AH). The benefits of the CS method are demonstrated using acoustic data acquired for a 22-in. scale-model fan stage run at the NASA Glenn Research Center's 9-foot by 15-foot wind tunnel. Two key outcomes of the work include (1) significant improvement in the spatial resolution of the measured sound field and (2) reduction in the overall data acquisition time. Additionally, the methods described here lead to new opportunities for noise source diagnostics and visualization.
C1 [Shah, Parthiv N.] ATA Engn Inc, San Diego, CA 92128 USA.
[Vold, Havard] ATA Engn Inc, Charleston, SC 29412 USA.
[Hensley, Dan] ATA Engn Inc, Lakewood, CO 80401 USA.
[Envia, Edmane; Stephens, David] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Shah, PN (reprint author), ATA Engn Inc, San Diego, CA 92128 USA.
NR 24
TC 0
Z9 0
U1 0
U2 0
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0889-504X
EI 1528-8900
J9 J TURBOMACH
JI J. Turbomach.-Trans. ASME
PD DEC
PY 2015
VL 137
IS 12
AR 121002
DI 10.1115/1.4031341
PG 11
WC Engineering, Mechanical
SC Engineering
GA DN5VD
UT WOS:000377138400002
ER
PT J
AU Le Vine, DM
Yueh, S
Brown, S
Lagerloef, GSE
Rabolli, M
AF Le Vine, David M.
Yueh, Simon
Brown, Shannon
Lagerloef, Gary S. E.
Rabolli, Monica
TI Foreword to the Special Issue on Status of Aquarius/SAC-D Mission
Calibration/Validation and Retrieval Algorithms
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Editorial Material
C1 [Le Vine, David M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yueh, Simon; Brown, Shannon] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Lagerloef, Gary S. E.] Earth & Space Res, Seattle, WA 98121 USA.
[Rabolli, Monica] Comis Nacl Actividades Espaciales CONAE, RA-1063 Buenos Aires, DF, Argentina.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5398
EP 5400
DI 10.1109/JSTARS.2016.2516064
PG 3
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700001
ER
PT J
AU Le Vine, DM
Dinnat, EP
Meissner, T
Yueh, SH
Wentz, FJ
Torrusio, SE
Lagerloef, G
AF Le Vine, David M.
Dinnat, Emmanuel P.
Meissner, Thomas
Yueh, Simon H.
Wentz, Frank J.
Torrusio, Sandra E.
Lagerloef, G.
TI Status of Aquarius/SAC-D and Aquarius Salinity Retrievals
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aquarius; L-band; microwave remote sensing; ocean salinity; radiometer
calibration
ID BAND RADIOMETER/SCATTEROMETER OBSERVATIONS; SEA-SURFACE SALINITY;
DIELECTRIC-CONSTANT; POLAR-REGIONS; MICROWAVE; RADIOMETER; SPACE;
INSTRUMENT; MISSION; SYSTEM
AB Aquarius was launched in June 2011 to monitor the global salinity field in the open ocean. This radiometer/scatterometer (i.e., passive/active) instrument is part of the Aquarius/SAC-D mission, a partnership between the USA and Argentina. In general, the observatory and instruments have functioned well with mostly minor issues. Aquarius has been operating successfully since being turned on August 25, 2011. The quality of the salinity retrieval has improved continuously and is approaching the accuracy goal of 0.2 psu (monthly global RMS). The maps produced by Aquarius show the global structure and dynamic features of the salinity field and, now after 3 years of operations, data are available to give a first look at the interannual changes in sea surface salinity. An improved salinity product, Version 3.0, has been released to the public (June 2014) and includes significant refinements in the retrieval algorithm such as reduced ascending/descending differences and improved calibration. Additional data such as global maps of soil moisture and maps of RFI are also available.
C1 [Le Vine, David M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dinnat, Emmanuel P.] Chapman Univ, Orange, CA 92866 USA.
[Dinnat, Emmanuel P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meissner, Thomas; Wentz, Frank J.] Remote Sensing Syst, Santa Rosa, CA 95401 USA.
[Yueh, Simon H.] Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA USA.
[Torrusio, Sandra E.] Comis Nacl Actividades Espaciales CONAE, SABIA Mar, Satellite Mission Argentine Space Agcy, C1063ACH Buenos Aires, Buenos Aires, DF, Argentina.
[Lagerloef, G.] Earth & Space Res, Seattle, WA 98121 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Dinnat, Emmanuel/D-7064-2012
OI Dinnat, Emmanuel/0000-0001-9003-1182
NR 47
TC 6
Z9 6
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5401
EP 5415
DI 10.1109/JSTARS.2015.2427159
PG 15
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700002
ER
PT J
AU Piepmeier, JR
Hong, L
Pellerano, FA
AF Piepmeier, Jeffrey R.
Hong, Liang
Pellerano, Fernando A.
TI Aquarius L-Band Microwave Radiometer: 3 Years of Radiometric Performance
and Systematic Effects
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Calibration; microwave radiometer
ID CALIBRATION; SALINITY; INSTRUMENT; STABILITY; ORBIT
AB The Aquarius L-band microwave radiometer is a three-beam pushbroom instrument designed to measure sea-surface salinity. Results are analyzed for performance and systematic effects over three years of operation. The thermal control system maintains tight temperature stability promoting good gain stability. The gain spectrum exhibits expected orbital variations with 1/f noise appearing at longer time periods. The on-board detection and integration scheme coupled with the calibration algorithm produce antenna temperatures with NEDT <0.16 K for 1.44-s samples. Nonlinearity is characterized before launch and the derived correction is verified with cold-sky calibration (CSC) data. Finally, long-term drift is discovered in all channels with 1-K amplitude and 100-day time constant. Nonetheless, it is adeptly corrected using an exponential model.
C1 [Piepmeier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Microwave Instrument Technol Branch, Greenbelt, MD 20771 USA.
[Hong, Liang] NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Laurel, MD 20723 USA.
[Pellerano, Fernando A.] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD 20771 USA.
RP Piepmeier, JR (reprint author), NASA, Goddard Space Flight Ctr, Microwave Instrument Technol Branch, Greenbelt, MD 20771 USA.; Hong, L (reprint author), NASA, Goddard Space Flight Ctr, Sci Applicat Int Corp, Laurel, MD 20723 USA.; Pellerano, FA (reprint author), NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD 20771 USA.
EM jeff.piepmeier@nasa.gov; liang.hong@nasa.gov;
Fernando.A.Pellerano@nasa.gov
RI Hong, Liang/D-3156-2017
OI Hong, Liang/0000-0002-8870-0399
NR 17
TC 1
Z9 1
U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5416
EP 5423
DI 10.1109/JSTARS.2015.2435493
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700003
ER
PT J
AU Fore, AG
Neumann, G
Freedman, AP
Chaubell, MJ
Tang, WQ
Hayashi, AK
Yueh, SH
AF Fore, Alexander G.
Neumann, Gregory
Freedman, Adam P.
Chaubell, Mario Julian
Tang, Wenqing
Hayashi, Akiko K.
Yueh, Simon H.
TI Aquarius Scatterometer Calibration
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aquarius; backscatter; L-band; ocean winds; radar; remote sensing;
scatterometery
ID WIND-SPEED; SALINITY
AB In this paper, we discuss the Aquarius scatterometer calibration, starting with the instrument calibration. We examine the stability of Aquarius as quantified using the loop-back power and estimated receiver gain to shown Aquarius has been extremely stable to order 0.1 dB since mission start. We show the temperatures of scatterometer components not contained in the loop-back path have been controlled precisely to 0.5 degrees C to minimize any temperature-dependent losses. Combined, these results show Aquarius produces accurate sigma(0) over the mission lifetime. In the next section, we discuss the stability as quantified using external models and again show stability to order 0.1 dB in very good agreement with instrument-only methods. Then, we discuss the methods used to absolutely calibrate Aquarius sigma(0) with respect to previous L-band radar systems. We show that Aquarius is relatively calibrated to order 0.1 dB for copolarization channels and better than 0.2 dB for cross-polarization channels. Finally, we discuss the calibration of the Aquarius wind speed product. We compare the Aquarius wind speed with radiometer wind speed products, other radar scatterometers, and numerical weather products. We show that the Aquarius wind speed product is on par with previous scatterometers in data quality.
C1 [Fore, Alexander G.; Neumann, Gregory; Freedman, Adam P.; Chaubell, Mario Julian; Tang, Wenqing; Hayashi, Akiko K.; Yueh, Simon H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Fore, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Fore@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. Government sponsorship acknowledged.
NR 14
TC 1
Z9 1
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5424
EP 5432
DI 10.1109/JSTARS.2015.2493449
PG 9
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700004
ER
PT J
AU Dinnat, EP
Le Vine, DM
Piepmeier, JR
Brown, ST
Hong, L
AF Dinnat, Emmanuel P.
Le Vine, David M.
Piepmeier, Jeffrey R.
Brown, Shannon T.
Hong, Liang
TI Aquarius L-band Radiometers Calibration Using Cold Sky Observations
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Antenna gain; antenna radiation patterns; calibration; microwave
radiometry; sea measurements
ID SURFACE SALINITY; SOIL-MOISTURE; MISSION; PARAMETERS; EMISSION; IMPACT
AB An important element in the calibration plan for the Aquarius radiometers is to look at the cold sky. This involves rotating the satellite 180 degrees from its nominal Earth viewing configuration to point the main beams at the celestial sky. At L-band, the cold sky provides a stable, well-characterized scene to be used as a calibration reference. This paper describes the cold sky calibration for Aquarius and how it is used as part of the absolute calibration. Cold sky observations helped establish the radiometer bias, by correcting for an error in the spillover lobe of the antenna pattern, and monitor the long-term radiometer drift.
C1 [Dinnat, Emmanuel P.] Chapman Univ, CEESMO, Orange, CA 92866 USA.
[Dinnat, Emmanuel P.; Le Vine, David M.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Piepmeier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD 20771 USA.
[Brown, Shannon T.] CALTECH, Jet Prop Lab, NASA, Microwave Syst, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hong, Liang] NASA, Goddard Space Flight Ctr, SAIC, Greenbelt, MD 20771 USA.
RP Dinnat, EP (reprint author), Chapman Univ, CEESMO, Orange, CA 92866 USA.; Dinnat, EP; Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.; Piepmeier, JR (reprint author), NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD 20771 USA.; Brown, ST (reprint author), CALTECH, Jet Prop Lab, NASA, Microwave Syst, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Hong, L (reprint author), NASA, Goddard Space Flight Ctr, SAIC, Greenbelt, MD 20771 USA.
EM emmanuel.dinnat@nasa.gov; david.m.levine@nasa.gov;
jeffrey.r.piepmeier@nasa.gov; shannon.t.brown@jpl.nasa.gov;
liang.hong@nasa.gov
RI Dinnat, Emmanuel/D-7064-2012; Hong, Liang/D-3156-2017
OI Dinnat, Emmanuel/0000-0001-9003-1182; Hong, Liang/0000-0002-8870-0399
FU National Aeronautics and Space Administration [NNX10AV23G]
FX This work was supported by the National Aeronautics and Space
Administration under Grant NNX10AV23G.
NR 35
TC 1
Z9 1
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5433
EP 5449
DI 10.1109/JSTARS.2015.2496362
PG 17
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700005
ER
PT J
AU Tang, WQ
Yueh, SH
Hayashi, A
Fore, AG
Jones, WL
Santos-Garcia, A
Jacob, MM
AF Tang, Wenqing
Yueh, Simon H.
Hayashi, Akiko
Fore, Alexander G.
Jones, W. Linwood
Santos-Garcia, Andrea
Marta Jacob, Maria
TI Rain-Induced Near Surface Salinity Stratification and Rain Roughness
Correction for Aquarius SSS Retrieval
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aquarius; L-band; rain effect; salinity retrieval; stratification
ID WIND RETRIEVAL; WATER CYCLE; OCEAN; MICROWAVE; MODEL; ARGO; VALIDATION;
CHALLENGE; DRIFTERS; SMOS
AB The effect of rain on surface salinity stratification is analyzed to develop a rain roughness correction scheme to reduce the uncertainty of Aquarius sea surface salinity (SSS) retrieved under rainy conditions. Rain freshwater inputs may cause large discrepancies in salinity measured by Aquarius at 1-2 cm within the surface and the calibration reference SSS from HYCOM (SSSHYCOM) a few meters below the surface. We used the rain impact model (RIM) to adjust SSSHYCOM to reflect near surface salinity stratification caused by freshwater inputs accumulated from rain events that occurred over the past 24 h before Aquarius measurements (SSSRIM). When calibrated with SSSRIM, the residuals, i.e., the difference between measured and model predicted brightness temperature T-B, are considered as rain-induced roughness. It was found that rain-induced roughness is larger at lower wind speeds, and decreases as wind increases. The Combined Active Passive algorithm is used to retrieve SSS with (SSSCAP_RC) or without (SSSCAP) rain roughness correction. We find that the simultaneously retrieved wind speed with rain roughness correction has significantly improved agreement with the NCEP wind speed with the rain-dependent bias reduced, self-justifying our rain correction approach. SSS retrieved is validated with salinity measured by drifters at a depth of 45 cm. The difference between satellite retrieved and in situ salinity increases with rain rate. With rain-induced roughness accounted for, the difference between satellite retrieval and drifter increases with rain rate with slope of -0.184 psu (mm h(-1))(-1), representing the salinity stratification between the two depths (1-2 cm versus 45 cm).
C1 [Tang, Wenqing; Yueh, Simon H.; Hayashi, Akiko; Fore, Alexander G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Jones, W. Linwood; Santos-Garcia, Andrea] Cent Florida Remote Sensing Lab, Orlando, FL 32816 USA.
[Marta Jacob, Maria] Ctr Espacial Teoilo Tabanera, Comis Nacl Actividades Espaciales, RA-5187 Falda Del Canete, Argentina.
RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Wenqing.Tang@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work described in this paper carried out by the authors at the Jet
Propulsion Laboratory, California Institute of Technology was performed
under a contract with the National Aeronautics and Space Administration.
The authors would like to thank three anonymous reviewers for their
comments for improving this paper.
NR 23
TC 0
Z9 0
U1 3
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5474
EP 5484
DI 10.1109/JSTARS.2015.2463768
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700009
ER
PT J
AU Yueh, SH
Tang, WQ
Fore, AG
Hayashi, A
AF Yueh, Simon H.
Tang, Wenqing
Fore, Alexander G.
Hayashi, Akiko
TI Impact of Ocean Wave Height on L-band Passive and Active Microwave
Observation of Sea Surfaces
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Microwave remote sensing; ocean wave; ocean wind; radar; radiometer
ID WIND-GENERATED WAVES; BRIGHTNESS TEMPERATURE; RADAR BACKSCATTER;
SALINITY; AQUARIUS; MODEL; SCATTEROMETRY; RETRIEVAL; MISSION; EMISSIVITY
AB The impact of ocean waves on L-band brightness temperatures and backscatter from the ocean surface was analyzed using Aquarius data. Matchups of Aquarius data with significant wave height (SWH) from National Oceanic and Atmospheric Administration (NOAA) WaveWatch3 reanalysis and the ocean surface wind are generated. We perform the analysis using two different wind speed products: special sensor microwave imager/sounder (SSMI/S) and National Center for Environmental Prediction (NCEP) operational data. Interestingly, the influence of SWH manifests itself differently for these two wind speed products. Conditionally, averaged normalized radar cross-section (sigma(0)) and brightness temperatures (T-B) by NCEP wind speed show strong influence by SWH over the entire range of NCEP wind speeds with a larger impact at lower wind speeds. However, performing the same analysis conditioned on the SSMI/S wind speed, the conclusion becomes entirely different: the SWH effects appear small at low wind speeds (<5 ms(-1)) and increase with increasing wind speed. The apparent contradiction is a result of the differing characteristics of NCEP and SSMI/S wind speeds. NCEP wind is an atmospheric model estimate of surface wind velocity, whereas the SSMI/S wind is a microwave remote sensing product, representing the characteristics of sea surface roughness. The impact of SWH needs to be considered when the SSMI/S wind speed is assimilated into the numerical weather prediction models, such as the NCEP.
C1 [Yueh, Simon H.; Tang, Wenqing; Fore, Alexander G.; Hayashi, Akiko] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Yueh, SH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM simon.yueh@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out by the Jet Propulsion Laboratory, California
Institute of Technology under a contract with the National Aeronautics
and Space Administration.
NR 33
TC 0
Z9 0
U1 2
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5491
EP 5499
DI 10.1109/JSTARS.2015.2432134
PG 9
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700011
ER
PT J
AU Hejazin, Y
Jones, WL
Santos-Garcia, A
Jacob, MM
El-Nimri, SF
AF Hejazin, Yazan
Jones, W. Linwood
Santos-Garcia, Andrea
Jacob, Maria Marta
El-Nimri, Salem Fawwaz
TI A Roughness Correction for Aquarius Sea Surface Salinity Using the CONAE
MicroWave Radiometer
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aquarius (AQ); ocean roughness; surface salinity
ID EARTH INCIDENCE ANGLES; OCEAN SURFACE; WIND SPEEDS; EMISSIVITY;
SCATTERING; VECTOR; RANGE; MODEL
AB Aquarius (AQ)/SAC-D is a joint National Aeronautics and Space Administration (NASA)/Comision Nacional de Actividades Espaciales (CONAE; Argentine Space Agency) Earth Sciences satellite mission to measure global sea surface salinity (SSS), using a L-band radiometer/scatterometer that measures ocean brightness temperature (Tb) and radar backscatter (sigma-0). The application of L-band radiometry to retrieve SSS is a difficult task; therefore, precise Tb corrections are necessary to obtain accurate measurements. One of the major error sources is the effect of ocean roughness that "warms" the ocean Tb. The baseline approach, to provide this ocean roughness correction, uses the AQ radar scatterometer measurement of ocean sigma-0 to infer the radiometric excess ocean emissivity. In contrast, this paper develops an alternate approach for the AQ ocean roughness correction using the MicroWave Radiometer (MWR) Tb measurements at Ka-band. The theoretical basis of this MWR ocean roughness correction algorithm is described, which translates these Ka-band measurements to L-band to remove the AQ Tb errors that are caused by ocean wind speed and direction. MWR ocean roughness correction results are compared with corresponding results from the AQ scatterometer method. Also, AQ SSS retrievals are presented using both sets of roughness corrections that demonstrate the relative effectiveness of the MWR and AQ scatterometer approaches.
C1 [Hejazin, Yazan; Jones, W. Linwood; Santos-Garcia, Andrea] Univ Cent Florida, Cent FL Remote Sensing Lab, Orlando, FL 32816 USA.
[Jacob, Maria Marta] CONAE, RA-5187 Falda Del Canete, Argentina.
[El-Nimri, Salem Fawwaz] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hejazin, Y (reprint author), Univ Cent Florida, Cent FL Remote Sensing Lab, Orlando, FL 32816 USA.
EM yazan.hejazin@gmail.com
FU NASA Headquarters Earth Science ROSES Program [NNX14AAI83G]
FX This research at CFRSL was performed with NASA Headquarters Earth
Science ROSES Program under Grant NNX14AAI83G for support of the AQ
Ocean SSS Science Team.
NR 26
TC 1
Z9 1
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD DEC
PY 2015
VL 8
IS 12
BP 5500
EP 5510
DI 10.1109/JSTARS.2015.2482491
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DE3HY
UT WOS:000370519700012
ER
PT J
AU Goldsmith, PF
Yildiz, UA
Langer, WD
Pineda, JL
AF Goldsmith, Paul F.
Yildiz, Umut A.
Langer, William D.
Pineda, Jorge L.
TI HERSCHEL GALACTIC PLANE SURVEY OF [N II] FINE STRUCTURE EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: general; ISM: structure
ID WARM IONIZED MEDIUM; RECOMBINATION LINE OBSERVATIONS; EFFECTIVE
COLLISION STRENGTHS; FAR-INFRARED SPECTROSCOPY; C-II; STAR-FORMATION;
PHYSICAL CONDITIONS; INNER GALAXY; INTERSTELLAR-MEDIUM; CARINA NEBULA
AB We present the first large-scale high angular resolution survey of ionized nitrogen in the Galactic Plane through emission of its two fine structure transitions ([N II]) at 122 and 205 mu m. The observations were largely obtained with the PACS instrument onboard the Herschel Space Observatory. The lines of sight were in the Galactic plane, following those of the Herschel OTKP project GOT C+. Both lines are reliably detected at the 10(-8)-10(-7) Wm(-2) sr(-1) level over the range -60 degrees <= l <= 60 degrees. The rms of the intensity among the 25 PACS spaxels of a given pointing is typically less than one third of the mean intensity, showing that the emission is extended. [N II] is produced in gas in which hydrogen is ionized, and collisional excitation is by electrons. The ratio of the two fine structure transitions provides a direct measurement of the electron density, yielding n(e) largely in the range 10-50 cm(-3) with an average value of 29 cm(-3) and N+ column densities 10(16)-10(17) cm(-2). [N II] emission is highly correlated with that of [C II], and we calculate that between 1/3 and 1/2 of the [C II] emission is associated with the ionized gas. The relatively high electron densities indicate that the source of the [N II] emission is not the warm ionized medium (WIM), which has electron densities more than 100 times smaller. Possible origins of the observed [N II] include the ionized surfaces of dense atomic and molecular clouds, the extended low-density envelopes of H II regions, and low-filling factor high-density fluctuations of the WIM.
C1 [Goldsmith, Paul F.; Yildiz, Umut A.; Langer, William D.; Pineda, Jorge L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paul.F.Goldsmith@jpl.nasa.gov
RI Yildiz, Umut/C-5257-2011; Goldsmith, Paul/H-3159-2016
OI Yildiz, Umut/0000-0001-6197-2864;
NR 63
TC 9
Z9 9
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 DEC 1
PY 2015
VL 814
IS 2
AR 133
DI 10.1088/0004-637X/814/2/133
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF6KA
UT WOS:000371463200002
ER
PT J
AU Lopez, LA
Grefenstette, BW
Reynolds, SP
An, HJ
Boggs, SE
Christensen, FE
Craig, WW
Eriksen, KA
Fryer, CL
Hailey, CJ
Harrison, FA
Madsen, KK
Stern, DK
Zhang, WW
Zoglauer, A
AF Lopez, Laura A.
Grefenstette, Brian W.
Reynolds, Stephen P.
An, Hongjun
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Eriksen, Kristoffer A.
Fryer, Chris L.
Hailey, Charles J.
Harrison, Fiona A.
Madsen, Kristin K.
Stern, Daniel K.
Zhang, William W.
Zoglauer, Andreas
TI A SPATIALLY RESOLVED STUDY OF THE SYNCHROTRON EMISSION AND TITANIUM IN
TYCHO'S SUPERNOVA REMNANT USING NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects: (Tycho's SNR); ISM: supernova remnants; X-rays:
ISM
ID GAMMA-RAY EMISSION; CHANDRASEKHAR MASS MODELS; CORE-COLLAPSE SUPERNOVAE;
LINE EMISSION; PARTICLE-ACCELERATION; NOVA REMNANTS; DOUBLE-DETONATION;
MOLECULAR CLOUD; MAGNETIC-FIELD; IA SUPERNOVAE
AB We report results from deep observations (similar to 750 ks) of Tycho's supernova remnant (SNR) with NuSTAR. Using these data, we produce narrow-band images over several energy bands to identify the regions producing the hardest X-rays and to search for radioactive decay line emission from Ti-44. We find that the hardest (>10 keV) X-rays are concentrated in the southwest of Tycho, where recent Chandra observations have revealed high emissivity "stripes" associated with particles accelerated to the knee of the cosmic-ray spectrum. We do not find evidence of Ti-44, and we set limits on its presence and distribution within the SNR. These limits correspond to an upper-limit Ti-44 mass of M-44 < 2.4 x 10(-4) M-circle dot for a distance of 2.3 kpc. We perform a spatially resolved spectroscopic analysis of 66 regions across Tycho. We map the best-fit rolloff frequency of the hard X-ray spectra, and we compare these results to measurements of the shock expansion and ambient density. We find that the highest energy electrons are accelerated at the lowest densities and in the fastest shocks, with a steep dependence of the rolloff frequency with shock velocity. Such a dependence is predicted by models where the maximum energy of accelerated electrons is limited by the age of the SNR rather than by synchrotron losses, but this scenario requires far lower magnetic field strengths than those derived from observations in Tycho. One way to reconcile these discrepant findings is through shock obliquity effects, and future observational work is necessary to explore the role of obliquity in the particle acceleration process.
C1 [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.
[Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Eriksen, Kristoffer A.; Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, Daniel K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lopez, LA (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
EM lopez.513@osu.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012;
Madsen, Kristin/0000-0003-1252-4891
FU NASA through Hubble Fellowship grant - Space Telescope Science Institute
[HST-HF2-51342.001]; NASA [NAS 5-26555, NNG08FD60C]
FX We acknowledge helpful discussions with Drs. Marco Miceli, Lorenzo
Sironi, and Patrick Slane. L.A.L. received support for this work from
NASA through Hubble Fellowship grant number HST-HF2-51342.001 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. Additionally, the work was supported under
NASA contract 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 NASA. We thank the NuSTAR
Operations, Software, and Calibration teams for support with the
execution and analysis of these observations. This research 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).
NR 74
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 DEC 1
PY 2015
VL 814
IS 2
AR 132
DI 10.1088/0004-637X/814/2/132
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF6KA
UT WOS:000371463200001
ER
PT J
AU Placek, B
Knuth, KH
Angerhausen, D
Jenkins, JM
AF Placek, Ben
Knuth, Kevin H.
Angerhausen, Daniel
Jenkins, Jon M.
TI CHARACTERIZATION OF KEPLER-91B AND THE INVESTIGATION OF A POTENTIAL
TROJAN COMPANION USING EXONEST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planets and satellites: detection; planets and
satellites: fundamental parameters; techniques: photometric
ID TRANSITING EXTRASOLAR PLANETS; SYSTEMATIC-ERROR CORRECTION; GIANT
PLANETS; BAYESIAN EVIDENCE; MODEL SELECTION; LIGHT CURVES; CANDIDATES;
EXOPLANETS; SEARCH; STARS
AB Presented here is an independent re-analysis of the Kepler light curve of Kepler-91 (KIC 8219268). Using the EXONEST software package, which provides both Bayesian parameter estimation and Bayesian model testing, we were able to re-confirm the planetary nature of Kepler-91b. In addition to the primary and secondary eclipses of Kepler-91b, a third dimming event appears to occur approximately 60 degrees away (in phase) from the secondary eclipse, leading to the hypothesis that a Trojan planet may be located at the L4 or L5 Lagrange points. Here, we present a comprehensive investigation of four possibilities to explain the observed dimming event using all available photometric data from the Kepler Space Telescope, recently obtained radial velocity measurements, and N-body simulations. We find that the photometric model describing Kepler-91b and a Trojan planet is highly favored over the model involving Kepler-91b alone. However, it predicts an unphysically high temperature for the Trojan companion, leading to the conclusion that the extra dimming event is likely a false-postive.
C1 [Placek, Ben; Knuth, Kevin H.] SUNY Albany, Dept Phys, Albany, NY 12222 USA.
[Angerhausen, Daniel] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Angerhausen, Daniel] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Placek, B (reprint author), SUNY Albany, Dept Phys, Albany, NY 12222 USA.
NR 45
TC 5
Z9 5
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 DEC 1
PY 2015
VL 814
IS 2
AR 147
DI 10.1088/0004-637X/814/2/147
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF6KA
UT WOS:000371463200016
ER
PT J
AU Schoeberl, MR
Jensen, EJ
Woods, S
AF Schoeberl, Mark R.
Jensen, Eric J.
Woods, Sarah
TI Gravity waves amplify upper tropospheric dehydration by clouds
SO EARTH AND SPACE SCIENCE
LA English
DT Article
ID TROPICAL TROPOPAUSE LAYER; STRATOSPHERIC WATER-VAPOR; DROPLET PROBE CDP;
ICE NUCLEATION; CIRRUS CLOUDS; AIRCRAFT OBSERVATIONS; PHYSICAL
PROCESSES; CRYSTAL NUMBERS; TEMPERATURE; PERFORMANCE
AB We use a 1-Dcloudmodel run using a prescribed temperature field to investigate the role of gravity waves in dehydration in the tropical tropopause layer (TTL). We find that gravity waves play an important role in the TTL dehydration process beyond just lowering the minimum temperature experienced by the air parcels. We show that the more rapid cooling in the presence of gravity waves significantly increases the abundance ice crystals. This increase in ice crystal concentration causes a more rapid depletion of vapor in excess of saturation, and the resultant cloud dehydration efficiency is increased. Using a spectrum of gravity waves, we generate ice particle statistics that are in good agreement with observations. We also find that the gravity waves increase cloudiness. Our results show that cloud physics and gravity wave temperature fluctuations cannot be neglected in simulating the TTL physics. In fact, it appears that short-period waves may be an essential component of the TTL cloud dehydration process.
C1 [Schoeberl, Mark R.] Sci & Technol Corp, Columbia, MD USA.
NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Woods, Sarah] SPEC Inc, Boulder, CO USA.
RP Schoeberl, MR (reprint author), Sci & Technol Corp, Columbia, MD USA.
EM mark.schoeberl@mac.com
NR 44
TC 2
Z9 2
U1 3
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 EARTH SPACE SCI
JI Earth Space Sci.
PD DEC
PY 2015
VL 2
IS 12
BP 485
EP 500
DI 10.1002/2015EA000127
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA DE6NP
UT WOS:000370751000001
ER
PT J
AU Gong, XB
Lydon, J
Cooper, K
Chou, K
AF Gong, Xibing
Lydon, James
Cooper, Kenneth
Chou, Kevin
TI CHARACTERIZATION OF Ti-6Al-4V POWDER IN ELECTRON BEAM MELTING ADDITIVE
MANUFACTURING
SO INTERNATIONAL JOURNAL OF POWDER METALLURGY
LA English
DT Article
ID MECHANICAL-PROPERTIES; THERMAL-CONDUCTIVITY; MICROSTRUCTURES
AB In this study, preheated Ti-6Al-4V powder from electron beam melting (EBM) additive manufacturing (AM) was characterized experimentally. In the EBM AM process, preheating serves to aggregate the precursor powder, lightly sintering it to prevent a spreading effect. Specimens with sintered Ti-6Al-4V powder enclosed were fabricated and prepared for microstructural and morphological examination using optical and scanning electron microscopy. Micro-CT scanning was conducted on the specimens and the results were analyzed to study the powder porosity and the powder-size distributions. In addition, the thermal conductivity of preheated powder from EBM AM was measured and analyzed at different temperatures. It was found that preheating results in metallurgical bonds or even partial melting of the powder. Neck formations are clearly evident in both the z-plane and x-plane samples. The diameter of the necks is about 1-10 mu m. In addition, micro-CT analysis confirms that a similar porosity level exists in both the z-plane and x-plane sections. The calculated porosity of the preheated powder is about 50%. The major diameter range of the powder is from 30-50 mu m. The Ti-6Al-4V powder has significantly lower thermal conductivity than that of a solid of the same chemical composition. The thermal conductivity of Ti-6Al-4V powder is also highly temperature dependent: about 0.63 W/m.K at room temperature and 2.44 W/m.K at 750 degrees C.
C1 [Gong, Xibing; Chou, Kevin] Univ Alabama, Dept Mech Engn, Box 870276, Tuscaloosa, AL 35487 USA.
[Lydon, James; Cooper, Kenneth] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Gong, XB (reprint author), Univ Alabama, Dept Mech Engn, Box 870276, Tuscaloosa, AL 35487 USA.
EM xgong2@crimson.ua.edu
FU NASA [NNX11AM11A]; AL EPSCoR GRSP
FX The materials presented in this paper are supported by NASA, under award
No. NNX11AM11A. The research is in collaboration with the Marshall Space
Flight Center, Advanced Manufacturing Team. In addition, Brandon
Walters, Rajaram Manoharan, and Benjamin Ache at Micro Photonics, Inc.,
assisted with micro-CT scans of Ti-6Al-4V EBM AM specimens. X.G. also
acknowledges the AL EPSCoR GRSP for their financial support.
NR 27
TC 2
Z9 3
U1 6
U2 12
PU AMER POWDER METALLURGY INST
PI PRINCETON
PA 105 COLLEGE ROAD EAST, PRINCETON, NJ 08540 USA
SN 0888-7462
J9 INT J POWDER METALL
JI Int. J. Powder Metall.
PD WIN
PY 2015
VL 51
IS 1
BP 25
EP 34
PG 10
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA DD8XZ
UT WOS:000370211500006
ER
PT J
AU Michell, RG
Janches, D
Samara, M
Hormaechea, JL
Brunini, C
Bibbo, I
AF Michell, R. G.
Janches, D.
Samara, M.
Hormaechea, J. L.
Brunini, C.
Bibbo, I.
TI Simultaneous optical and radar observations of meteor head-echoes
utilizing SAAMER
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Meteor; Optical; Head echo; Meteor mass
ID LIDAR OBSERVATIONS; UPPER-ATMOSPHERE; INPUT FUNCTION; HIGH-POWER; MU
RADAR; METHODOLOGY; ABLATION; MASS; TRAILS; MODEL
AB We present simultaneous optical and radar observations of meteors observed with the Southern Argentine Agile MEteor Radar (SAAMER). Although such observations were performed in the past using High Power and Large Aperture radars, the focus here is on meteors that produced head echoes that can be detected by a significantly less sensitive but more accessible radar system. An observational campaign was conducted in August of 2011, where an optical imager was operated near the radar site in Rio Grande, Tierra del Fuego, Argentina. Six head echo events out of 150 total detections were identified where simultaneous optical meteors could also be clearly seen within the main radar beam. The location of the meteors derived from the radar interferometry agreed very well with the optical location, verifying the accuracy of the radar interferometry technique. The meteor speeds and origin directions calculated from the radar data were accurate compared with the optics for the 2 meteors that had radar signal-to-noise ratios above 2.5. The optical meteors that produced the head echoes had horizontal velocities in the range of 29-91 km/s. These comparisons with optical observations improve the accuracy of the radar detection and analysis techniques, such that, when applied over longer periods of time, will improve the statistics of southern hemisphere meteor observations. Mass estimates were derived using both the optical and radar data and the resulting masses agreed well with each other. All were within an order of magnitude and in most cases, the agreement was within a factor of two. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Michell, R. G.] Univ Maryland, College Pk, MD 20742 USA.
[Michell, R. G.; Janches, D.; Samara, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Tierra Del Fueg, Argentina.
[Brunini, C.; Bibbo, I.] Natl Univ La Plata, Dept Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina.
RP Michell, RG (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM robertg.michell@nasa.gov
RI Janches, Diego/D-4674-2012;
OI Janches, Diego/0000-0001-8615-5166; Hormaechea, Jose
Luis/0000-0003-4533-3282
FU Southwest Research Institute; NSF [AGS-1456161, AGS-1456129,
AGS-0944104, AST-0908118]; NASA [12-PAST12-0007, 12-PATM12-0006]
FX The research was funded in part by Southwest Research Institute internal
research and development grant. R.M. is supported by NSF Grants
AGS-1456161 and AGS-1456129. SAAMER is supported by NSF awards
AGS-0944104 and AST-0908118. DJ. is supported by NASA awards
12-PAST12-0007 and 12-PATM12-0006. The authors would like to thank
Jonathan Yee and Stephen Pifko for their assistance in the observational
campaign as well as all the staff at Estacion Astronomica Rio Grande for
their generosity and hospitality. We thank N. Swarnalingam for his
assistance in determining the radar derived masses.
NR 39
TC 3
Z9 3
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC 1
PY 2015
VL 118
SI SI
BP 95
EP 101
DI 10.1016/j.pss.2015.04.018
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE2LZ
UT WOS:000370460100012
ER
PT J
AU Zubko, E
Videen, G
Hines, DC
Shkuratov, Y
Kaydash, V
Muinonen, K
Knight, MM
Sitko, ML
Lisse, CM
Mutchler, M
Wooden, DH
Li, JY
Kobayashi, H
AF Zubko, Evgenij
Videen, Gorden
Hines, Dean C.
Shkuratov, Yuriy
Kaydash, Vadym
Muinonen, Karri
Knight, Matthew M.
Sitko, Michael L.
Lisse, Carey M.
Mutchler, Max
Wooden, Diane H.
Li, Jian-Yang
Kobayashi, Hiroshi
TI Cornet C/2012 S1 (ISON) coma composition at similar to 4 au from HST
observations
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
ID O1 HALE-BOPP; HUBBLE-SPACE-TELESCOPE; OPTICAL-CONSTANTS; COMETARY DUST;
IMAGING POLARIMETRY; SILICATE MINERALOGY; REFRACTIVE-INDEXES;
INFRARED-SPECTRA; LIGHT-SCATTERING; 81P/WILD-2 DUST
AB We analyze the first color and polarization images of Comet ISON (C/2012 S1) taken during two measurement campaigns of the Hubble Space Telescope (HST) on UTC 2013 April 10 and May 8, when the phase angles of Comet ISON were alpha approximate to 13.7 degrees and 12.2 degrees, respectively. We model the particles in the coma using highly irregular agglomerated debris particles. Even though the observations were made over a small range of phase angle, the data still place significant constraints on the material properties of the cometary coma. The different photo-polarimetric responses are indicative of spatial chemical heterogeneity of coma in Comet ISON. For instance, at small projected distances to the nucleus (< 500 km), our modeling suggests the cometary particles are composed predominantly of small, highly absorbing particles, such as amorphous carbon and/or organics material heavily irradiated with UV radiation; whereas, at longer projected distances (> 1000 km), the refractive index of the particles is consistent with organic matter slightly processed with UV radiation, tholins, Mg-Fe silicates, and/or Mg-rich silicates contaminated with similar to 10% (by volume) amorphous carbon. The modeling suggests low relative abundances of particles with low material absorption in the visible, i.e., Im(m) <= 0.02. Such particles were detected unambiguously in other comets in the vicinity of nucleus through very strong negative polarization near backscattering (P approximate to -6%) and very low positive polarization (P approximate to 3-5%) at side scattering. These materials were previously attributed to Mg-rich silicates forming a refractory surface layer on the surface of cometary nuclei (Zubko et al., 2012). The absence of such particles in Comet ISON could imply an absence of such a layer on its nucleus. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Zubko, Evgenij; Shkuratov, Yuriy; Kaydash, Vadym] Kharkov Natl Univ, Inst Astron, 35 Sumskaya St, UA-61022 Kharkov, Ukraine.
[Videen, Gorden; Hines, Dean C.; Sitko, Michael L.] Space Sci Inst, Boulder, CO 80301 USA.
[Videen, Gorden; Mutchler, Max] INTA, Madrid 28850, Spain.
[Videen, Gorden] Univ Cantabria, Fac Ciencias, Dept Fis Aplicada, Grp Opt, E-39005 Santander, Spain.
[Videen, Gorden] US Army Res Lab, Adelphi, MD 20783 USA.
[Hines, Dean C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Muinonen, Karri] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
[Muinonen, Karri] Finnish Geospatial Res Inst, FI-02431 Masala, Finland.
[Knight, Matthew M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Knight, Matthew M.; Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Wooden, Diane H.] NASA Ames Res Ctr, Mountain View, CA USA.
[Li, Jian-Yang] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Kobayashi, Hiroshi] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
RP Zubko, E (reprint author), Kharkov Natl Univ, Inst Astron, 35 Sumskaya St, UA-61022 Kharkov, Ukraine.
EM evgenij.s.zubko@gmail.com
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Zubko, Evgenij/0000-0001-9994-923X
FU NASA from Space Telescope Science Institute [GO 13199]; NASA
[NAS5-26555]
FX This work was partially supported through program number GO 13199
provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555.
NR 86
TC 4
Z9 4
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC 1
PY 2015
VL 118
SI SI
BP 138
EP 163
DI 10.1016/j.pss.2015.08.002
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DE2LZ
UT WOS:000370460100018
ER
PT J
AU Moon, JH
Song, YT
Lee, H
AF Moon, Jae-Hong
Song, Y. Tony
Lee, HuiKyo
TI PDO and ENSO modulations intensified decadal sea level variability in
the tropical Pacific
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE regional sea level; tropical Pacific; PDO-ENSO relationship
ID EL-NINO; OCEAN; CLIMATE; EVENTS; REANALYSIS; FREQUENCY; MONSOON; TRENDS;
IMPACT; SIGNAL
AB According to long-term sea level reconstruction and steric sea level data, regional sea levels in the tropical Pacific have oscillated between east and west on a decadal time scale over the past 60 years, but the oscillation has been intensified significantly in the last three decades. Using conditional composite analysis, we show that the recent intensification in sea level variability is caused by modulation between the Pacific Decadal Oscillation (PDO) and El Nino-Southern Oscillation (ENSO), i.e., an El Nino in a positive PDO or a La Nina in a negative PDO phase. Our analysis of meteorological fields indicates that atmospheric circulation associated with the changes in ENSO-PDO phase relationship plays a positive role in enhancing the decadal sea level oscillation. The intensified sea level oscillation, when superimposed on the global trend of sea level rise, will have profound implications for coastal communities, therefore, the combined effect of PDO and ENSO should be taken into account in the decadal sea level prediction in the tropical Pacific.
C1 [Moon, Jae-Hong] Jeju Natl Univ, Dept Earth & Marine Sci, Jejusi, South Korea.
[Song, Y. Tony; Lee, HuiKyo] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Moon, JH (reprint author), Jeju Natl Univ, Dept Earth & Marine Sci, Jejusi, South Korea.
EM jhmoon@jejunu.ac.kr
FU National Institute of Supercomputing and Network/Korea Institute of
Science and Technology Information [KSC-2014-C1-050]
FX H. Lee was supported by the Jet Propulsion Laboratory's Data Science
Initiative. This research is carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA). This work was
partly supported by the National Institute of Supercomputing and
Network/Korea Institute of Science and Technology Information with
supercomputing resources including technical support (KSC-2014-C1-050).
Data for the atmospheric fields are available at Earth System Research
Laboratory. Data set: NCEP/NCAR Reanalysis. The SSL data are available
at the National Center for Atmospheric Research (NCAR), Computational
and Information Systems Laboratory. Data set:
http://rda.ucar.edu/datasets/ds285.3/. Many thanks to B. D. Hamlington
and B. Meyssignac for providing their long-term sea level reconstruction
data.
NR 37
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U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD DEC
PY 2015
VL 120
IS 12
BP 8229
EP 8237
DI 10.1002/2015JC011139
PG 9
WC Oceanography
SC Oceanography
GA DC3XO
UT WOS:000369153200028
ER
PT J
AU Boardsen, SA
Jian, LK
Raines, JL
Gershman, DJ
Zurbuchen, TH
Roberts, DA
Korth, H
AF Boardsen, S. A.
Jian, L. K.
Raines, J. L.
Gershman, D. J.
Zurbuchen, T. H.
Roberts, D. A.
Korth, H.
TI MESSENGER survey of in situ low frequency wave storms between 0.3 and
0.7 AU
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ION-CYCLOTRON WAVES; SOLAR-WIND; ELECTROMAGNETIC-WAVES; DIFFERENTIAL
FLOW; MAGNETIC HELICITY; ALPHA-PARTICLES; PROTON; CORONA; FLUCTUATIONS;
GENERATION
AB MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) magnetometer data was surveyed between 0.3 and 0.7 AU from 6 June 2007 to 23 March 2011 for low-frequency wave (LFW) storms, when the magnetometer was sampling at a rate of at least 2 s(-1). A total of 12,197 LFW events were identified, of which 5506 lasted 10 min or longer. The events have a high degree of polarization, are circularly polarized, with wave vectors nearly aligned or antialigned with the interplanetary magnetic field (IMF) at frequencies in the vicinity of the proton cyclotron frequency. These events are observed about 6% of the time, preferentially associated with radially directed inward or outward IMF. Their occurrence rate and median duration do not change much with R, where R is the heliocentric radial distance. For a narrow-frequency window in the solar wind frame, left-handed storms in the spacecraft frame have a power drop off that is roughly proportional to R-3 which is consistent with a source close the Sun, while right-handed storms have a power drop off roughly proportional R-1 which is not consistent with a source close to the Sun. The power in the left-handed LFW storms is on average greater than the right-handed ones by a factor of 3. In the solar wind frame, the wave frequency decreases from 0.13 to 0.04 Hz moving from 0.3 to 0.7 AU, but the frequency normalized by the local proton cyclotron frequency does not change much with the running median varying from 0.35 to 0.5. The normalized frequency band widths of the wave power spectra increase slightly with R, possibly associated with energy dissipation.
C1 [Boardsen, S. A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Boardsen, S. A.; Jian, L. K.; Roberts, D. A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Jian, L. K.; Gershman, D. J.] Univ Maryland, Goddard Planetary Heliophys Inst, College Pk, MD 20742 USA.
[Raines, J. L.; Zurbuchen, T. H.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Gershman, D. J.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Boardsen, SA (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
EM scott.a.boardsen@nasa.gov
RI Jian, Lan/B-4053-2010
OI Jian, Lan/0000-0002-6849-5527
FU NASA [NNX13AI65G, NNX15AB75G]
FX The MESSENGER data used in this study were obtained from the Planetary
Data System at http://pds.nasa.gov/. The OMNI data were obtained from
the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. This
work is supported by NASA research grants NNX13AI65G and NNX15AB75G.
NR 26
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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 DEC
PY 2015
VL 120
IS 12
BP 10207
EP 10220
DI 10.1002/2015JA021506
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC4GZ
UT WOS:000369180200006
ER
PT J
AU Ream, JB
Walker, RJ
Ashour-Abdalla, M
El-Alaoui, M
Wiltberger, M
Kivelson, MG
Goldstein, ML
AF Ream, J. B.
Walker, R. J.
Ashour-Abdalla, M.
El-Alaoui, M.
Wiltberger, M.
Kivelson, M. G.
Goldstein, M. L.
TI Propagation of Pi2 pulsations through the braking region in global MHD
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID BURSTY BULK FLOWS; MAGNETIC PULSATIONS; NUMERICAL-SIMULATION; GEOTAIL
OBSERVATIONS; AURORAL STREAMERS; SUBSTORM ONSETS; PI-2 PULSATIONS;
ELECTRIC-FIELDS; PLASMA SHEET; GROWTH-PHASE
AB We investigate the propagation of Pi2 period pulsations from their origin in the plasma sheet through the braking region, the region where the fast flows are slowed as they approach the inner edge of the plasma sheet. Our approach is to use both the University of California, Los Angeles (UCLA) and Lyon-Fedder-Mobarry (LFM) global magnetohydrodynamic (MHD) computer codes to simulate the Earth's magnetosphere during a substorm that occurred on 14 September 2004 when Pi2 pulsations were observed. We use two different MHD models in order to test the robustness of our conclusions about Pi2. The simulations are then compared with ground-based and satellite data. We find that the propagation of the pulsations in the simulations, especially through the braking region, depends strongly on the ionospheric models used at the inner boundary of the MHD models. With respect to typical observed values, the modeled conductances are high in the UCLA model and low in the LFM model. The different conductances affect the flows, producing stronger line tying that slows the flow in the braking region more in the UCLA model than in the LFM model. Therefore, perturbations are able to propagate much more freely into the inner magnetosphere in the LFM results. However, in both models Pi2 period perturbations travel with the dipolarization front (DF) that forms at the earthward edge of the flow channel, but as the DF slows in the braking region, -8 <= x <= -6 R-E, the Pi2 period perturbations begin to travel ahead of it into the inner magnetosphere. This indicates that the flow channels generate compressional waves with periods that fall within the Pi2 range and that, as the flows themselves are stopped in the braking region, the compressional wave continues to propagate into the inner magnetosphere.
C1 [Ream, J. B.; Walker, R. J.; Kivelson, M. G.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Ashour-Abdalla, M.; El-Alaoui, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Kivelson, M. G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD USA.
RP Ream, JB (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
EM jodiebt@ucla.edu
RI Wiltberger, Michael/B-8781-2008
OI Wiltberger, Michael/0000-0002-4844-3148
FU NASA [NNX09AV91G, NNX13AE39G]; NASA Graduate Student Research Program
through Goddard Space Flight Center [NNX10AM08H]; Magnetospheric
Multiscale project through an Interdisciplinary Science grant; UCLA
(NASA) [NNX08AO48G]; NSF [AGS-1265967]; NASA grant UCB/NASA [NAS
5-02099]; National Science Foundation [OCI-1053575]
FX This work was supported by NASA grant NNX09AV91G. This research was also
supported in part by the NASA Graduate Student Research Program through
Goddard Space Flight Center, grant NNX10AM08H. M.L. Goldstein and M.
Ashour-Abdalla were supported by the Magnetospheric Multiscale project
through an Interdisciplinary Science grant to the Goddard Space Flight
Center and UCLA (NASA grant NNX08AO48G at UCLA). M. El-Alaoui was
supported by NSF grant AGS-1265967. M.G. Kivelson was supported by NASA
grant UCB/NASA NAS 5-02099. M. Wiltberger was supported by NASA grant
NNX13AE39G. The National Center for Atmospheric Research is sponsored by
the National Science Foundation. We would like to acknowledge
high-performance computing support from Yellowstone
(ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information
Systems Laboratory, sponsored by the National Science Foundation.
Computational resources for the UCLA model were provided by the Extreme
Science and Engineering Discovery Environment (XSEDE), which is
supported by National Science Foundation grant OCI-1053575. All
satellite and OMNI data were obtained through the Virtual Magnetospheric
Observatory (VMO) (http://vmo.igpp.ucla.edu/). We acknowledge the
experiment teams that acquired, processed, and provided the
OMNI-included data, and J.H. King and N.E. Papitashvili of NASA/GSFC for
creating the OMNI data set. Geotail magnetic field data were provided by
T. Nagai, JAXA in Japan. We acknowledge C. Carr and the Double Star TC1
FGM instrument team, as well as ESA, Double Star, Center for Space
Science and Applied Research, and the Chinese Academy of Sciences for
Double Star data. We also acknowledge the World Data Center for
Geomagnetism, Kyoto (http://wdc.kugi.kyoto-u.ac.jp/index.html) and the
Geomagnetic Network of China, for Pi2 data. We thank Krishan Khurana,
Tung-Shin Hsu, and Robert J. Strangeway for helpful discussions during
the course of this research.
NR 63
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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 DEC
PY 2015
VL 120
IS 12
BP 10574
EP 10591
DI 10.1002/2015JA021572
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC4GZ
UT WOS:000369180200029
ER
PT J
AU McCanta, MC
Hatfield, RG
Thomson, BJ
Hook, SJ
Fisher, E
AF McCanta, Molly C.
Hatfield, Robert G.
Thomson, Bradley J.
Hook, Simon J.
Fisher, Elizabeth
TI Identifying cryptotephra units using correlated rapid, nondestructive
methods: VSWIR spectroscopy, X-ray fluorescence, and magnetic
susceptibility
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE tephrochronology; cryptotephra; identification; spectroscopy; magnetic
susceptibility
ID SOUFRIERE HILLS VOLCANO; QUATERNARY TEPHRA LAYERS; MARINE SEDIMENT
CORES; LESSER-ANTILLES; NORTH-ATLANTIC; NEW-ZEALAND; LATE PLEISTOCENE;
DISTAL TEPHRA; REFLECTANCE SPECTRA; ERUPTION HISTORY
AB Understanding the frequency, magnitude, and nature of explosive volcanic eruptions is essential for hazard planning and risk mitigation. Terrestrial stratigraphic tephra records can be patchy and incomplete due to subsequent erosion and burial processes. In contrast, the marine sedimentary record commonly preserves a more complete historical record of volcanic activity as individual events are archived within continually accumulating background sediments. While larger tephra layers are often identifiable by changes in sediment color and/or texture, smaller fallout layers may also be present that are not visible to the naked eye. These cryptotephra are commonly more difficult to identify and often require time-consuming and destructive point counting, petrography, and microscopy work. Here we present several rapid, nondestructive, and quantitative core scanning methodologies (magnetic susceptibility, visible to shortwave infrared spectroscopy, and XRF core scanning) which, when combined, can be used to identify the presence of increased volcaniclastic components (interpreted to be cryptotephra) in the sedimentary record. We develop a new spectral parameter (BDI1000VIS) that exploits the absorption of the 1 mu m near-infrared band in tephra. Using predetermined mixtures, BDI1000VIS can accurately identify tephra layers in concentrations >15-20%. When applied to the upper approximate to 270 kyr record of IODP core U1396C from the Caribbean Sea, and verified by traditional point counting, 29 potential cryptotephra layers were identified as originating from eruptions of the Lesser Antilles Volcanic Arc. Application of these methods in future coring endeavors can be used to minimize the need for physical disaggregation of valuable drill core material and allow for near-real-time recognition of tephra units, both visible and cryptotephra.
C1 [McCanta, Molly C.; Fisher, Elizabeth] Tufts Univ, Dept Earth & Ocean Sci, Medford, MA 02155 USA.
[Hatfield, Robert G.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Thomson, Bradley J.] Boston Univ, Ctr Remote Sensing, Boston, MA 02215 USA.
[Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP McCanta, MC (reprint author), Tufts Univ, Dept Earth & Ocean Sci, Medford, MA 02155 USA.
EM molly.mccanta@tufts.edu
RI Hook, Simon/D-5920-2016
OI Hook, Simon/0000-0002-0953-6165
FU NSF [EAR-1347868, EAR-1347912, OCE-1260671]
FX The authors acknowledge IODP Expedition 340 for core collection and
initial cataloging. The manuscript was greatly improved in revision,
thanks to the careful and critical reviews of M. Cassidy and Editor U.
Faul. We also thank R. Milliken and K. Robertson for assistance
collecting the initial spectral data of the core end-member
constituents. We note that there are no data sharing issues since all of
the numerical information resulting from the techniques applied in this
paper is provided in the figures. This paper was supported by NSF grants
EAR-1347868 to M.C.M., EAR-1347912 and OCE-1260671 to R.G.H., and
EAR-1347868 to B.J.T.
NR 101
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U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD DEC
PY 2015
VL 16
IS 12
BP 4029
EP 4056
DI 10.1002/2015GC005913
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DB9CO
UT WOS:000368814000001
ER
PT J
AU Arnold, NP
Randall, DA
AF Arnold, Nathan P.
Randall, David A.
TI Global-scale convective aggregation: Implications for the Madden-Julian
Oscillation
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE aggregation; MJO; entrainment; RCE
ID TROPICAL INTRASEASONAL VARIABILITY; STATIC ENERGY BUDGET;
TEMPERATURE-GRADIENT APPROXIMATION; COMMUNITY ATMOSPHERE MODEL;
WATER-VAPOR; CLIMATE SENSITIVITY; SELF-AGGREGATION; PARAMETERIZATION
CRCP; CUMULUS CONVECTION; CLOUD-RADIATION
AB Previous work has shown that convection will self-organize in cloud-system-resolving model simulations of radiative-convective equilibrium, and it has been suggested that the convective envelope of the Madden-Julian oscillation (MJO) may be organized by similar processes on a much larger scale. Here we present support for that hypothesis based on simulations with SP-CAM with globally uniform SST. Without rotation, convection self-organizes into large (approximate to 4000 km) clusters surrounded by dry regions, while with Earth-like rotation the model produces a robust MJO. The nonrotating aggregation and MJO are found to have similar budgets of moist static energy, both being supported by diabatic feedbacks, particularly cloud-longwave interaction. Mechanism denial experiments show that longwave heating anomalies associated with high clouds are essential to the nonrotating aggregation, and amplify the MJO. Simulations using the conventional CAM show a weaker MJO and a much weaker tendency for nonrotating aggregation, and both MJO activity and aggregation intensity are found to increase with the entrainment rate in the deep convection parameterization.
C1 [Arnold, Nathan P.; Randall, David A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Arnold, NP (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
EM nathan.arnold@nasa.gov
RI Randall, David/E-6113-2011
OI Randall, David/0000-0001-6935-4112
FU National Science Foundation (USA) Science and Technology Center for
Multi-Scale Modeling of Atmospheric Processes [AGS-0425247]; NOAA
Climate and Global Change postdoctoral fellowship; National Science
Foundation through XSEDE resources
FX The authors thank Bjorn Stevens and an anonymous reviewer for insightful
comments that improved the manuscript. This work was supported by the
National Science Foundation (USA) Science and Technology Center for
Multi-Scale Modeling of Atmospheric Processes, managed by Colorado State
University under cooperative agreement AGS-0425247. N.P.A. was supported
by a NOAA Climate and Global Change postdoctoral fellowship. The model
computations were carried out on the Stampede cluster at the University
of Texas at Austin, supported by the National Science Foundation through
XSEDE resources. The model output is archived and available by request.
NR 66
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U1 4
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD DEC
PY 2015
VL 7
IS 4
BP 1499
EP 1518
DI 10.1002/2015MS000498
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB8AW
UT WOS:000368739800001
ER
PT J
AU Daleu, CL
Plant, RS
Woolnough, SJ
Sessions, S
Herman, MJ
Sobel, A
Wang, S
Kim, D
Cheng, A
Bellon, G
Peyrille, P
Ferry, F
Siebesma, P
van Ulft, L
AF Daleu, C. L.
Plant, R. S.
Woolnough, S. J.
Sessions, S.
Herman, M. J.
Sobel, A.
Wang, S.
Kim, D.
Cheng, A.
Bellon, G.
Peyrille, P.
Ferry, F.
Siebesma, P.
van Ulft, L.
TI Intercomparison of methods of coupling between convection and
large-scale circulation: 1. Comparison over uniform surface conditions
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE tropical convection; large-scale parameterized dynamics;
weak-temperature gradient; damped gravity wave; multiple equilibria
ID RESOLVING MODEL SIMULATIONS; TEMPERATURE-GRADIENT APPROXIMATION;
LARGE-EDDY SIMULATION; DEEP CONVECTION; CUMULUS CONVECTION;
BOUNDARY-LAYERS; SINGLE-COLUMN; TROPICAL PRECIPITATION; VERTICAL
DIFFUSION; SCHEME DESCRIPTION
AB As part of an international intercomparison project, a set of single-column models (SCMs) and cloud-resolving models (CRMs) are run under the weak-temperature gradient (WTG) method and the damped gravity wave (DGW) method. For each model, the implementation of the WTG or DGW method involves a simulated column which is coupled to a reference state defined with profiles obtained from the same model in radiative-convective equilibrium. The simulated column has the same surface conditions as the reference state and is initialized with profiles from the reference state. We performed systematic comparison of the behavior of different models under a consistent implementation of the WTG method and the DGW method and systematic comparison of the WTG and DGW methods in models with different physics and numerics. CRMs and SCMs produce a variety of behaviors under both WTG and DGW methods. Some of the models reproduce the reference state while others sustain a large-scale circulation which results in either substantially lower or higher precipitation compared to the value of the reference state. CRMs show a fairly linear relationship between precipitation and circulation strength. SCMs display a wider range of behaviors than CRMs. Some SCMs under the WTG method produce zero precipitation. Within an individual SCM, a DGW simulation and a corresponding WTG simulation can produce different signed circulation. When initialized with a dry troposphere, DGW simulations always result in a precipitating equilibrium state. The greatest sensitivities to the initial moisture conditions occur for multiple stable equilibria in some WTG simulations, corresponding to either a dry equilibrium state when initialized as dry or a precipitating equilibrium state when initialized as moist. Multiple equilibria are seen in more WTG simulations for higher SST. In some models, the existence of multiple equilibria is sensitive to some parameters in the WTG calculations.
C1 [Daleu, C. L.; Plant, R. S.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Woolnough, S. J.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Sessions, S.; Herman, M. J.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM USA.
[Sobel, A.] Columbia Univ, Dept Environm Sci, New York, NY USA.
[Wang, S.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Kim, D.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Cheng, A.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA.
[Bellon, G.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Peyrille, P.; Ferry, F.] Meteo France, Toulouse, France.
[Siebesma, P.; van Ulft, L.] Royal Netherlands Meteorol Inst, POB 201, NL-3730 AE De Bilt, Netherlands.
[Siebesma, P.] Delft Univ Technol, Delft, Netherlands.
RP Daleu, CL (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM c.daleu@reading.ac.uk
RI Wang, Shuguang/C-2893-2011; Sobel, Adam/K-4014-2015;
OI Wang, Shuguang/0000-0003-1861-9285; Sobel, Adam/0000-0003-3602-0567;
Bellon, Gilles/0000-0003-3981-1225
FU NERC [NE/K004034/1]; National Centre for Atmospheric Science, a NERC
collaborative center; U.S. National Science Foundation [AGS-1056254,
AGS-1342001, 1342001]; NM EPSCoR; NSF [AGS-1062206]; NASA [NNX13AM18G];
Korea Meteorological Administration Research and Development Program
[CATER 2013-3142]; DOE Atmospheric System Research Program
[DE-SC0005450, DE-SC0008779]; European Commissions [282672]
FX C.L.D., R.S.P., and S.J.W. thank the UK Met Office for the availability
of the LEM at version 2.4 and SCM version 7.8 of the UK Met Office
Unified Model. C.L.D. was supported by NERC, grant NE/K004034/1. S.J.W.
was supported by the National Centre for Atmospheric Science, a NERC
collaborative center. The New Mexico Tech group thanks Carlos Lopez
Carrillo, Ana Juracic, and Stipo Sentic for model output analysis and
for continual discussions on the tropical atmosphere. We also thank Raul
Morales-Juberias for use of the Pelican beowulf cluster. S.L.S.
acknowledges support from U.S. National Science Foundation grants
AGS-1056254 and AGS-1342001 and NM EPSCoR. M.J.H. was supported by U.S.
National Science Foundation grant 1342001. A.H.S. and S.W. were
partially supported by NSF grant AGS-1062206. The WRF simulations were
carried out on the Yeti Shared HPC Cluster at Columbia University. G.B.
thanks Isabelle Beau, Antoinette Alias, David Saint Martin, Jean-Yves
Grandpeix, Marie-Pierre Lefebvre, and the CNRS/INSU-LEFE project DEPHY
and the European Union FP7 project EMBRACE. D.K. appreciates the
NASA/GISS modeling group, especially Maxwell Kelley, Mao-Sung Yao, and
Anthony Del Genio, for their invaluable and unlimited supports. D.K. and
A.H.S. was supported by the NASA grant NNX13AM18G and the Korea
Meteorological Administration Research and Development Program under
grant CATER 2013-3142. LaRC CRM-IPHOC was partially supported by DOE
Atmospheric System Research Program under Interagency agreements
DE-SC0005450 and DE-SC0008779. The computation resources were provided
by SSAI Icluster and LaRC Kcluster. P.P., A.P.S., and L.U. were
supported by the European Commissions Seventh Framework Programme, under
grant agreement 282672, EMBRACE project. Data used for this research are
available upon request from the corresponding author; please send
requests via email to c.daleu@reading.ac.uk.
NR 78
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U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD DEC
PY 2015
VL 7
IS 4
BP 1576
EP 1601
DI 10.1002/2015MS000468
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB8AW
UT WOS:000368739800005
ER
PT J
AU Li, HY
Leung, LR
Tesfa, T
Voisin, N
Hejazi, M
Liu, L
Liu, Y
Rice, J
Wu, H
Yang, XF
AF Li, Hong-Yi
Leung, L. Ruby
Tesfa, Teklu
Voisin, Nathalie
Hejazi, Mohamad
Liu, Lu
Liu, Ying
Rice, Jennie
Wu, Huan
Yang, Xiaofan
TI Modeling stream temperature in the Anthropocene: An earth system
modeling approach
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE stream temperature; earth system modeling; reservoir operation
ID INTEGRATED ASSESSMENT; CLIMATE-CHANGE; ELECTRICITY-GENERATION; WATER;
21ST-CENTURY; PROJECTIONS; DEMANDS; SURFACE
AB A new large-scale stream temperature model has been developed within the Community Earth System Model (CESM) framework. The model is coupled with the Model for Scale Adaptive River Transport (MOSART) that represents river routing and a water management model (WM) that represents the effects of reservoir operations and water withdrawals on flow regulation. The coupled models allow the impacts of reservoir operations and withdrawals on stream temperature to be explicitly represented in a physically based and consistent way. The models have been applied to the Contiguous United States driven by observed meteorological forcing. Including water management in the models improves the agreement between the simulated and observed streamflow at a large number of stream gauge stations. It is then shown that the model is capable of reproducing stream temperature spatiotemporal variation satisfactorily by comparing against the observed data from over 320 USGS stations. Both climate and water management are found to have important influence on the spatiotemporal patterns of stream temperature. Furthermore, it is quantitatively estimated that reservoir operation could cool down stream temperature in the summer low-flow season (August-October) by as much as 1 approximate to 2 degrees C due to enhanced low-flow conditions, which have important implications to aquatic ecosystems. Sensitivity of the simulated stream temperature to input data and reservoir operation rules used in the WM model motivates future directions to address some limitations in the current modeling framework.
C1 [Li, Hong-Yi; Leung, L. Ruby; Tesfa, Teklu; Voisin, Nathalie; Hejazi, Mohamad; Liu, Ying; Rice, Jennie; Yang, Xiaofan] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Liu, Lu; Wu, Huan] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Wu, Huan] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Li, HY (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA.
EM hongyi.li@pnnl.gov
RI Li, Hong-Yi/C-9143-2014;
OI Li, Hong-Yi/0000-0001-5690-3610; Voisin, Nathalie/0000-0002-6848-449X
FU Office of Science of the U.S. Department of Energy Biological and
Environmental Research as part of the Integrated Assessment Research
Program; Battelle for the U.S. Department of Energy [DE-AC05-76RLO1830]
FX This work was supported by the Office of Science of the U.S. Department
of Energy Biological and Environmental Research as part of the
Integrated Assessment Research Program. Initial model development and
compilation of observation data for model evaluation were supported by
the Platform for Regional Integrated Modeling and Analysis (PRIMA)
initiative at the Pacific Northwest National Laboratory. The Pacific
Northwest National Laboratory is operated by Battelle for the U.S.
Department of Energy under Contract DE-AC05-76RLO1830. The data and
source code used in this study are available upon individual request
(hongyi.li@pnnl.gov).
NR 36
TC 0
Z9 0
U1 3
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD DEC
PY 2015
VL 7
IS 4
BP 1661
EP 1679
DI 10.1002/2015MS000471
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB8AW
UT WOS:000368739800009
ER
PT J
AU Benafan, O
Chen, SY
Kar, A
Vaidyanathan, R
AF Benafan, O.
Chen, S. -Y.
Kar, A.
Vaidyanathan, R.
TI Laser surface modification of medical grade alloys for reduced heating
in a magnetic resonance imaging environment
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID METALLIC IMPLANTS; MRI; DIFFUSION
AB Nanoscale surface modification of medical grade metallic alloys was conducted using a neodymiumdoped yttrium aluminum garnet laser-based dopant diffusion technique. The objective of this approach was to minimize the induction heating by reducing the absorbed radio frequency field. Such an approach is advantageous in that the dopant is diffused into the alloy and is not susceptible to detachment or spallation as would an externally applied coating, and is expected to not deteriorate the mechanical and electrical properties of the base alloy or device. Experiments were conducted using a controlled environment laser system with the ability to control laser properties (i.e., laser power, spot size, and irradiation time) and dopant characteristics (i.e., temperature, concentration, and pressure). The reflective and transmissive properties of both the doped and untreated samples were measured in a radio frequency (63.86 MHz) magnetic field using a system comprising a high power signal generator, a localized magnetic field source and sensor, and a signal analyzer. The results indicate an increase in the reflectivity of the laser-treated samples compared to untreated samples. The effect of reflectivity on the heating of the alloys is investigated through a mathematical model incorporating Maxwell's equations and heat conduction. (C) 2015 AIP Publishing LLC.
C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Mech & Aerosp Engn, Mat Sci & Engn, AMPAC, Orlando, FL 32816 USA.
[Chen, S. -Y.; Kar, A.] Univ Cent Florida, Coll Opt & Photon, CREOL, Laser Adv Mat Proc Lab, Orlando, FL 32816 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov; raj@ucf.edu
NR 22
TC 0
Z9 0
U1 1
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD DEC
PY 2015
VL 86
IS 12
AR 123903
DI 10.1063/1.4936970
PG 9
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA DB6AG
UT WOS:000368594900045
PM 26724043
ER
PT J
AU Giles, BL
AF Giles, Barbara L.
TI Annual Forum Raises Awareness Across the Space Weather Enterprise
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Giles, Barbara L.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Giles, Barbara L.] NASA, Goddard Space Flight Ctr, MMS Fast Plasma Invest, Greenbelt, MD USA.
RP Giles, BL (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.; Giles, BL (reprint author), NASA, Goddard Space Flight Ctr, MMS Fast Plasma Invest, Greenbelt, MD USA.
EM barbara.giles@nasa.gov
NR 0
TC 0
Z9 0
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 DEC
PY 2015
VL 13
IS 12
BP 826
EP 826
DI 10.1002/2015SW001338
PG 1
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DC3ZM
UT WOS:000369159300003
ER
PT J
AU Gordeev, E
Sergeev, V
Honkonen, I
Kuznetsova, M
Rastatter, L
Palmroth, M
Janhunen, P
Toth, G
Lyon, J
Wiltberger, M
AF Gordeev, E.
Sergeev, V.
Honkonen, I.
Kuznetsova, M.
Rastaetter, L.
Palmroth, M.
Janhunen, P.
Toth, G.
Lyon, J.
Wiltberger, M.
TI Assessing the performance of community-available global MHD models using
key system parameters and empirical relationships
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; ART.; MAGNETOSPHERE; CONVECTION;
SIMULATION; VARIABILITY; DIRECTION; STRENGTH; GEOTAIL; CODE
AB Global magnetohydrodynamic (MHD) modeling is a powerful tool in space weather research and predictions. There are several advanced and still developing global MHD (GMHD) models that are publicly available via Community Coordinated Modeling Center's (CCMC) Run on Request system, which allows the users to simulate the magnetospheric response to different solar wind conditions including extraordinary events, like geomagnetic storms. Systematic validation of GMHD models against observations still continues to be a challenge, as well as comparative benchmarking of different models against each other. In this paper we describe and test a new approach in which (i) a set of critical large-scale system parameters is explored/tested, which are produced by (ii) specially designed set of computer runs to simulate realistic statistical distributions of critical solar wind parameters and are compared to (iii) observation-based empirical relationships for these parameters. Being tested in approximately similar conditions (similar inputs, comparable grid resolution, etc.), the four models publicly available at the CCMC predict rather well the absolute values and variations of those key parameters (magnetospheric size, magnetic field, and pressure) which are directly related to the large-scale magnetospheric equilibrium in the outer magnetosphere, for which the MHD is supposed to be a valid approach. At the same time, the models have systematic differences in other parameters, being especially different in predicting the global convection rate, total field-aligned current, and magnetic flux loading into the magnetotail after the north-south interplanetary magnetic field turning. According to validation results, none of the models emerges as an absolute leader. The new approach suggested for the evaluation of the models performance against reality may be used by model users while planning their investigations, as well as by model developers and those interesting to quantitatively evaluate progress in magnetospheric modeling.
C1 [Gordeev, E.; Sergeev, V.] St Petersburg State Univ, St Petersburg 199034, Russia.
[Honkonen, I.; Palmroth, M.; Janhunen, P.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Honkonen, I.; Kuznetsova, M.; Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Toth, G.] Univ Michigan, Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Lyon, J.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Gordeev, E (reprint author), St Petersburg State Univ, St Petersburg 199034, Russia.
EM evgeny.i.gordeev@spbu.ru
RI Wiltberger, Michael/B-8781-2008; Toth, Gabor/B-7977-2013; Gordeev,
Evgeny/H-8222-2013; Sergeev, Victor/H-1173-2013
OI Wiltberger, Michael/0000-0002-4844-3148; Toth,
Gabor/0000-0002-5654-9823; Gordeev, Evgeny/0000-0002-2687-7287; Sergeev,
Victor/0000-0002-4569-9631
FU Russian Science Foundation [14-17-00072]
FX This work was supported by the Russian Science Foundation grant
14-17-00072. Model computations were performed at the Community
Coordinated Modeling Center, NASA GSFC. The authors wish to acknowledge
the rest of the CCMC staff for their generous support throughout the
work discussed in the paper. We also thank M. Kholeva for her help in
the paper preparation.
NR 39
TC 4
Z9 4
U1 1
U2 4
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 DEC
PY 2015
VL 13
IS 12
BP 868
EP 884
DI 10.1002/2015SW001307
PG 17
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DC3ZM
UT WOS:000369159300007
ER
PT J
AU Carmack, E
Polyakov, I
Padman, L
Fer, I
Hunke, E
Hutchings, J
Jackson, J
Kelley, D
Kwok, R
Layton, C
Melling, H
Perovich, D
Persson, O
Ruddick, B
Timmermans, ML
Toole, J
Ross, T
Vavrus, S
Winsor, P
AF Carmack, E.
Polyakov, I.
Padman, L.
Fer, I.
Hunke, E.
Hutchings, J.
Jackson, J.
Kelley, D.
Kwok, R.
Layton, C.
Melling, H.
Perovich, D.
Persson, O.
Ruddick, B.
Timmermans, M. -L.
Toole, J.
Ross, T.
Vavrus, S.
Winsor, P.
TI TOWARD QUANTIFYING THE INCREASING ROLE OF OCEANIC HEAT IN SEA ICE LOSS
IN THE NEW ARCTIC
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID HORIZONTAL DENSITY STRUCTURE; ATLANTIC WATER; BOUNDARY CURRENT; FRAM
STRAIT; INTERNAL WAVES; BEAUFORT SEA; YERMAK PLATEAU; PACIFIC WATER;
SURFACE-LAYER; CANADA BASIN
AB The loss of Arctic sea ice has emerged as a leading signal of global warming. This, together with acknowledged impacts on other components of the Earth system, has led to the term the new Arctic. Global coupled climate models predict that ice loss will continue through the twenty-first century, with implications for governance, economics, security, and global weather. A wide range in model projections reflects the complex, highly coupled interactions between the polar atmosphere, ocean, and cryosphere, including teleconnections to lower latitudes. This paper summarizes our present understanding of how heat reaches the ice base from the original sourcesinflows of Atlantic and Pacific Water, river discharge, and summer sensible heat and shortwave radiative fluxes at the ocean/ice surfaceand speculates on how such processes may change in the new Arctic. The complexity of the coupled Arctic system, and the logistic and technological challenges of working in the Arctic Ocean, require a coordinated interdisciplinary and international program that will not only improve understanding of this critical component of global climate but will also provide opportunities to develop human resources with the skills required to tackle related problems in complex climate systems. We propose a research strategy with components that include 1) improved mapping of the upper- and middepth Arctic Ocean, 2) enhanced quantification of important process, 3) expanded long-term monitoring at key heat-flux locations, and 4) development of numerical capabilities that focus on parameterization of heat-flux mechanisms and their interactions.
C1 [Carmack, E.] Fisheries & Oceans Canada, Sidney, BC, Canada.
[Carmack, E.] Univ Alaska Fairbanks, Coll Nat Sci & Math, Fairbanks, AK USA.
[Polyakov, I.] Univ Alaska Fairbanks, Int Arct Res Ctr, Fairbanks, AK USA.
[Polyakov, I.] Univ Alaska Fairbanks, Coll Nat Sci & Math, Fairbanks, AK USA.
[Padman, L.] Earth & Space Res, Corvallis, OR USA.
[Fer, I.] Univ Bergen, Inst Geophys, Bergen, Norway.
[Fer, I.] Univ Bergen, Bjerknes Ctr Climate Res, Bergen, Norway.
[Hunke, E.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Hutchings, J.] Oregon State Univ, Corvallis, OR 97331 USA.
[Jackson, J.] Hakai Inst, Heriot Bay, BC, Canada.
[Kelley, D.; Layton, C.; Ruddick, B.] Dalhousie Univ, Halifax, NS, Canada.
[Kwok, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Melling, H.] Fisheries & Oceans Canada, Sidney, BC, Canada.
[Perovich, D.] US Army, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA.
[Persson, O.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Timmermans, M. -L.] Yale Univ, New Haven, CT USA.
[Toole, J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Vavrus, S.] Univ Wisconsin, Ctr Climat Res, Madison, WI USA.
[Winsor, P.] Univ Alaska Fairbanks, Inst Marine Sci, Fairbanks, AK USA.
RP Polyakov, I (reprint author), UAF, IARC, POB 757335, Fairbanks, AK 99775 USA.
EM igor@iarc.uaf.edu
RI Kwok, Ron/A-9762-2008;
OI Kwok, Ron/0000-0003-4051-5896; Jackson, Jennifer/0000-0002-2318-8814
FU IARC; College of Natural Science and Mathematics, University of Alaska
Fairbanks
FX The document reflects contributions and discussions from a Sydney
Chapman Chair workshop entitled "An Untersteiner Workshop: On the Role
and Consequences of Ocean Heat Flux in Sea Ice Melt," held 19-21 March
2013 at the International Arctic Research Center (IARC) at the
University of Alaska Fairbanks. We deeply appreciate the logistics
support offer by L. Hinzman, and staff of IARC, and financial support
provided by IARC and by the College of Natural Science and Mathematics,
University of Alaska Fairbanks.
NR 219
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U1 12
U2 38
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD DEC
PY 2015
VL 96
IS 12
BP 2079
EP 2105
DI 10.1175/BAMS-D-13-00177.1
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB4RP
UT WOS:000368501100001
ER
PT J
AU Otto, FEL
Coelho, CAS
King, A
De Perez, EC
Wada, Y
van Oldenborgh, GJ
Haarsma, R
Haustein, K
Uhe, P
van Aalst, M
Aravequia, JA
Almeida, W
Cullen, H
AF Otto, Friederike E. L.
Coelho, Caio A. S.
King, Andrew
De Perez, Erin Coughlan
Wada, Yoshihide
van Oldenborgh, Geert Jan
Haarsma, Rein
Haustein, Karsten
Uhe, Peter
van Aalst, Maarten
Aravequia, Jose Antonio
Almeida, Waldenio
Cullen, Heidi
TI FACTORS OTHER THAN CLIMATE CHANGE, MAIN DRIVERS OF 2014/15 WATER
SHORTAGE IN SOUTHEAST BRAZIL
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Otto, Friederike E. L.; Haustein, Karsten; Uhe, Peter] Univ Oxford, Environm Change Inst, Oxford, England.
[Coelho, Caio A. S.; Aravequia, Jose Antonio; Almeida, Waldenio] Natl Inst Space Res INPE, Ctr Weather Forecast & Climate Studies CPTEC, Sao Paulo, Brazil.
[King, Andrew] Univ Melbourne, Sch Earth Sci, ARC Ctr Excellence Climate Syst Sci, Melbourne, Vic, Australia.
[De Perez, Erin Coughlan] Red Cross Red Crescent Climate Ctr, The Hague, Netherlands.
[De Perez, Erin Coughlan] Vrije Univ Amsterdam, Inst Environm Studies IVM, Amsterdam, Netherlands.
[De Perez, Erin Coughlan] Int Res Inst Climate & Soc, Palisades, NY USA.
[Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands.
[Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[van Oldenborgh, Geert Jan; Haarsma, Rein] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
[van Aalst, Maarten] Red Cross Red Crescent Climate Ctr, The Hague, Netherlands.
[van Aalst, Maarten] Int Res Inst Climate & Soc, Palisades, NY USA.
[Cullen, Heidi] Climate Cent, Princeton, NJ USA.
RP Otto, FEL (reprint author), Univ Oxford, Environm Change Inst, Oxford, England.
FU EUCLEIA project - European Union
FX We thank Antonio Divino Moura and David Karoly for their guidance and
input on the manuscript and Dina Sperling and Roop Singh for all their
help, our colleagues at the Oxford eResearch Centre and the Met Office
Hadley Centre PRECIS team for their support for the application and
development of weather@home and all participants in
climateprediction.net. The work was supported by the EUCLEIA project
funded by the European Union's Seventh Framework Programme
[FP7/2007-2013].
NR 15
TC 5
Z9 5
U1 3
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD DEC
PY 2015
VL 96
IS 12
BP S35
EP S40
DI 10.1175/BAMS-D-15-00120.1
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DB4SL
UT WOS:000368503300008
ER
PT J
AU Yoder, MR
Schultz, KW
Heien, EM
Rundle, JB
Turcotte, DL
Parker, JW
Donnellan, A
AF Yoder, Mark R.
Schultz, Kasey W.
Heien, Eric M.
Rundle, John B.
Turcotte, Donald L.
Parker, Jay W.
Donnellan, Andrea
TI The Virtual Quake earthquake simulator: a simulation-based forecast of
the El Mayor-Cucapah region and evidence of predictability in simulated
earthquake sequences
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Persistence, memory, correlations, clustering; Probabilistic
forecasting; Self-organization; Seismic cycle; Earthquake interaction,
forecasting and prediction; Statistical seismology
ID SOUTHERN-CALIFORNIA; ROCK FRACTURE; BRITTLE ROCK; FAULT MODEL;
PREDICTION; SEISMICITY; PRECURSORS; BEHAVIOR; PROBABILITIES; NUCLEATION
AB In this manuscript, we introduce a framework for developing earthquake forecasts using Virtual Quake (VQ), the generalized successor to the perhaps better known Virtual California (VC) earthquake simulator. We discuss the basic merits and mechanics of the simulator, and we present several statistics of interest for earthquake forecasting. We also show that, though the system as a whole (in aggregate) behaves quite randomly, (simulated) earthquake sequences limited to specific fault sections exhibit measurable predictability in the form of increasing seismicity precursory to large m > 7 earthquakes. In order to quantify this, we develop an alert-based forecasting metric, and show that it exhibits significant information gain compared to random forecasts. We also discuss the long-standing question of activation versus quiescent type earthquake triggering. We show that VQ exhibits both behaviours separately for independent fault sections; some fault sections exhibit activation type triggering, while others are better characterized by quiescent type triggering. We discuss these aspects of VQ specifically with respect to faults in the Salton Basin and near the El Mayor-Cucapah region in southern California, USA and northern Baja California Norte, Mexico.
C1 [Yoder, Mark R.; Schultz, Kasey W.; Rundle, John B.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Heien, Eric M.; Rundle, John B.; Turcotte, Donald L.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
[Rundle, John B.] Santa Fe Inst, Santa Fe, NM 87501 USA.
[Parker, Jay W.; Donnellan, Andrea] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yoder, MR (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
EM mryoder@ucdavis.edu
FU NASA Earth and Space Science fellowship [NNX11AL92H]; NASA [NNX08AF69G];
JPL [1291967]
FX This research is supported by the NASA Earth and Space Science
fellowship number NNX11AL92H, NASA grant NNX08AF69G and JPL Subcontract
1291967.
NR 85
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U1 3
U2 8
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 DEC
PY 2015
VL 203
IS 3
BP 1587
EP 1604
DI 10.1093/gji/ggv320
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DB3QQ
UT WOS:000368426800008
ER
PT J
AU Han, J
Brearley, AJ
Keller, LP
AF Han, Jangmi
Brearley, Adrian J.
Keller, Lindsay P.
TI Microstructural evidence for a disequilibrium condensation origin for
hibonite-spinel inclusions in the ALHA77307 CO3.0 chondrite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MURCHISON CARBONACEOUS CHONDRITE; REFRACTORY INCLUSIONS; RICH
INCLUSIONS; CO CHONDRITES; METEORITE; ANOMALIES; GRAINS; CM; EFREMOVKA;
CORUNDUM
AB Two hibonite-spinel inclusions (CAIs 03 and 08) in the ALHA77307 CO3.0 chondrite have been characterized in detail using the focused ion beam sample preparation technique combined with transmission electron microscopy. These hibonite-spinel inclusions are irregularly shaped and porous objects and consist of randomly oriented hibonite laths enclosed by aggregates of spinel with fine-grained perovskite inclusions finally surrounded by a partial rim of diopside. Melilite is an extremely rare phase in this type of CAI and occurs only in one inclusion (CAI 03) as interstitial grains between hibonite laths and on the exterior of the inclusion. The overall petrologic and mineralogical observations suggest that the hibonite-spinel inclusions represent high-temperature condensates from a cooling nebular gas. The textural relationships indicate that hibonite is the first phase to condense, followed by perovskite, spinel, and diopside. Texturally, melilite condensation appears to have occurred after spinel, suggesting that the condensation conditions were far from equilibrium. The crystallographic orientation relationships between hibonite and spinel provide evidence of epitaxial nucleation and growth of spinel on hibonite surfaces, which may have lowered the activation energy for spinel nucleation compared with that of melilite and consequently inhibited melilite condensation. Hibonite contains abundant stacking defects along the (001) plane consisting of different ratios of the spinel and Ca-containing blocks within the ideal hexagonal hibonite structure. This modification of the stacking sequence is likely the result of accommodation of excess Al in the gas into hibonite due to incomplete condensation of corundum from a cooling gas under disequilibrium conditions. We therefore conclude that these two hibonite-spinel inclusions in ALHA77307 formed by high-temperature condensation under disequilibrium conditions.
C1 [Han, Jangmi; Brearley, Adrian J.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Han, Jangmi] USRA, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Han, Jangmi; Keller, Lindsay P.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Han, J (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
EM jangmi.han@nasa.gov
FU NASA [NNG06GG37G, NNX12AH59G, 10-COS10-0049]; State of New Mexico;
National Science Foundation; NASA
FX We thank Dr. Denton Ebel and Dr. Rhonda Stroud for their helpful and
constructive reviews and Dr. Ed Scott for his comments and editorial
handling. The Antarctic Meteorite Working Group is thanked for the loan
of the sample of ALHA77307 from the Antarctic Meteorite Collection. This
work was supported by NASA grants NNG06GG37G and NNX12AH59G (A. J.
Brearley, P.I.) and 10-COS10-0049 (L. P. Keller, P.I.). Electron
microprobe analysis was carried out in the Electron Microbeam Analysis
Facility, Department of Earth and Planetary Sciences and Institute of
Meteoritics at the University of New Mexico. The facility is supported
by funds from the State of New Mexico, the National Science Foundation,
and NASA. We are grateful to Mike Spilde for his assistance with
electron microprobe analyses and Dr. Ying-Bing Jiang for his assistance
with TEM analyses. LPI contribution No. 1867.
NR 47
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U1 3
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD DEC
PY 2015
VL 50
IS 12
BP 2121
EP 2136
DI 10.1111/maps.12563
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DA7XJ
UT WOS:000368018600010
ER
PT J
AU Agnello, A
Treu, T
Ostrovski, F
Schechter, PL
Buckley-Geer, EJ
Lin, H
Auger, MW
Courbin, F
Fassnacht, CD
Frieman, J
Kuropatkin, N
Marshall, PJ
McMahon, RG
Meylan, G
More, A
Suyu, SH
Rusu, CE
Finley, D
Abbott, T
Abdalla, FB
Allam, S
Annis, J
Banerji, M
Benoit-Levy, A
Bertin, E
Brooks, D
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Cunha, CE
D'Andrea, CB
da Costa, LN
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Eifler, TF
Estrada, J
Neto, AF
Flaugher, B
Fosalba, P
Gerdes, DW
Gruen, D
Gutierrez, G
Honscheid, K
James, DJ
Kuehn, K
Lahav, O
Lima, M
Maia, MAG
March, M
Marshall, JL
Martini, P
Melchior, P
Miller, CJ
Miquel, R
Nichol, RC
Ogando, R
Plazas, AA
Reil, K
Romer, AK
Roodman, A
Sako, M
Sanchez, E
Santiago, B
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Tucker, D
Walker, AR
Wechsler, RH
Zhang, Y
AF Agnello, A.
Treu, T.
Ostrovski, F.
Schechter, P. L.
Buckley-Geer, E. J.
Lin, H.
Auger, M. W.
Courbin, F.
Fassnacht, C. D.
Frieman, J.
Kuropatkin, N.
Marshall, P. J.
McMahon, R. G.
Meylan, G.
More, A.
Suyu, S. H.
Rusu, C. E.
Finley, D.
Abbott, T.
Abdalla, F. B.
Allam, S.
Annis, J.
Banerji, M.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Burke, D. L.
Carnero Rosell, A.
Kind, M. Carrasco
Carretero, J.
Cunha, C. E.
D'Andrea, C. B.
da Costa, L. N.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Eifler, T. F.
Estrada, J.
Fausti Neto, A.
Flaugher, B.
Fosalba, P.
Gerdes, D. W.
Gruen, D.
Gutierrez, G.
Honscheid, K.
James, D. J.
Kuehn, K.
Lahav, O.
Lima, M.
Maia, M. A. G.
March, M.
Marshall, J. L.
Martini, P.
Melchior, P.
Miller, C. J.
Miquel, R.
Nichol, R. C.
Ogando, R.
Plazas, A. A.
Reil, K.
Romer, A. K.
Roodman, A.
Sako, M.
Sanchez, E.
Santiago, B.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Tucker, D.
Walker, A. R.
Wechsler, R. H.
Zhang, Y.
TI Discovery of two gravitationally lensed quasars in the Dark Energy
Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; methods: observational; methods:
statistical; quasars: emission lines
ID BROAD-LINE REGION; TIME DELAYS; MATTER SUBSTRUCTURE; IMAGING SURVEYS;
ACCRETION DISK; GALAXIES; FIELD; SELECTION; SEARCH
AB We present spectroscopic confirmation of two new gravitationally lensed quasars, discovered in the Dark Energy Survey (DES) and Wide-field Infrared Survey Explorer (WISE) based on their multiband photometry and extended morphology in DES images. Images of DES J0115-5244 show a red galaxy with two blue point sources at either side, which are images of the same quasar at z(s) = 1.64 as obtained by our long-slit spectroscopic data. The Einstein radius estimated from the DES images is 0.51 arcsec. DES J2146-0047 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fibre spectrum shows a quasar component at z(s) = 2.38 and absorption by Mg Pi and Fe Pi at z(1) = 0.799, which we tentatively associate with the foreground lens galaxy. Our long-slit spectra show that the blue components are resolved images of the same quasar. The Einstein radius is 0.68 arcsec, corresponding to an enclosed mass of 1.6 x 10(11) M-circle dot. Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data mining and model-based selection that is being applied to the entire DES data set.
C1 [Agnello, A.; Treu, T.] PAB, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Ostrovski, F.; Auger, M. W.; McMahon, R. G.; Banerji, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ostrovski, F.; McMahon, R. G.; Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Ostrovski, F.] Minist Educ Brazil, CAPES Fdn, BR-70040020 Brasilia, DF, Brazil.
[Schechter, P. L.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Buckley-Geer, E. J.; Lin, H.; Frieman, J.; Kuropatkin, N.; Finley, D.; Allam, S.; Annis, J.; Diehl, H. T.; Estrada, J.; Flaugher, B.; Gutierrez, G.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.; Tucker, D.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Courbin, F.; Meylan, G.] EPFL, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland.
[Fassnacht, C. D.; Rusu, C. E.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Marshall, P. J.; Burke, D. L.; Reil, K.; Roodman, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94035 USA.
[More, A.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Suyu, S. H.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile.
[Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Bertin, E.] Inst Astrophys, CNRS, 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.; Cunha, C. E.; Roodman, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Kind, M. Carrasco; Sevilla-Noarbe, I.; Thaler, J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Carretero, J.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[D'Andrea, C. B.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Desai, S.; Dietrich, J. P.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Desai, S.; Dietrich, J. P.] Univ Munich, Fac Phys, D-81679 Munich, Germany.
[Eifler, T. F.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Univ Munich, Univ Sternwarte, Fak Phys, D-81679 Munich, Germany.
[Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, BR-05314970 Sao Paulo, SP, Brazil.
[Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain.
[Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
RP Agnello, A (reprint author), PAB, Dept Phys & Astron, 430 Portola Plaza,Box 951547, Los Angeles, CA 90095 USA.
EM aagnello@astro.ucla.edu; tt@astro.ucla.edu
RI Ogando, Ricardo/A-1747-2010; Lima, Marcos/E-8378-2010; Sanchez,
Eusebio/H-5228-2015; Fosalba Vela, Pablo/I-5515-2016; Sobreira,
Flavia/F-4168-2015; EPFL, Physics/O-6514-2016;
OI Ogando, Ricardo/0000-0003-2120-1154; Sanchez,
Eusebio/0000-0002-9646-8198; Sobreira, Flavia/0000-0002-7822-0658;
Dietrich, Jorg/0000-0002-8134-9591; Carrasco Kind,
Matias/0000-0002-4802-3194; McMahon, Richard/0000-0001-8447-8869;
Abdalla, Filipe/0000-0003-2063-4345; Tucker, Douglas/0000-0001-7211-5729
FU NSF [AST-1312329, AST-1450141, AST-1138766, , ]; Packard
Foundation through a Packard Research Fellowship; Ministry of Science
and Technology in Taiwan [MOST-103- 2112-M-001-003-MY3]; Swiss National
Science Foundation (SNSF); US Department of Energy [DE-AC02-76SF00515];
DOE; NSF (USA); MISE (Spain); STFC (UK); HEFCE (UK); NCSA (UIUC); KICP
(U. Chicago); CCAPP (Ohio State); MIFPA (Texas AM); CNPQ; FAPERJ; FINEP
(Brazil); MINECO (Spain); DFG (Germany); Collaborating Institutions in
the Dark Energy Survey; MINECO [AYA2012-39559, ESP2013-48274,
FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERC
under the EU's 7th Framework Programme including grants ERC [240672,
291329, 306478]
FX This Letter includes data gathered with the 6.5m Baade Telescopes
located at Las Campanas Observatory, Chile. AA, TT, CDF and CER
acknowledge support from NSF grants AST-1312329 and AST-1450141
'Collaborative Research: Accurate cosmology with strong gravitational
lens time delays'. AA and TT gratefully acknowledge support by the
Packard Foundation through a Packard Research Fellowship to TT. SHS
acknowledges support from the Ministry of Science and Technology in
Taiwan via grant MOST-103- 2112-M-001-003-MY3. FC and GM are supported
by the Swiss National Science Foundation (SNSF). The work of PJM was
supported by the US Department of Energy under contract number
DE-AC02-76SF00515. We thank Tamara Davis, Cristina Furlanetto, Gary
Bernstein and Tom Collett for useful comments on earlier versions of
this Letter.; This Letter has gone through internal review by the DES
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. The Collaborating Institutions
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. The DES Data
Management System is supported by the NSF under grant number
AST-1138766. 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 ERC
under the EU's 7th Framework Programme including grants ERC 240672,
291329 and 306478.
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 1
PY 2015
VL 454
IS 2
BP 1260
EP 1265
DI 10.1093/mnras/stv2171
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7PZ
UT WOS:000367997700007
ER
PT J
AU Graham, ML
Nugent, PE
Sullivan, M
Filippenko, AV
Cenko, SB
Silverman, JM
Clubb, KI
Zheng, W
AF Graham, M. L.
Nugent, P. E.
Sullivan, M.
Filippenko, A. V.
Cenko, S. B.
Silverman, J. M.
Clubb, K. I.
Zheng, W.
TI Constraining the progenitor companion of the nearby Type Ia SN 2011fe
with a nebular spectrum at+981 d
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; supernovae: individual: SN 2011fe
ID SINGLE-DEGENERATE SCENARIO; SUPERNOVA EXPLOSIONS; STAR; SPECTROSCOPY;
TELESCOPE; EVOLUTION; HELIUM; SUBTRACTION; ENVIRONMENT; HYDROGEN
AB We present an optical nebular spectrum of the nearby Type Ia supernova 2011fe, obtained 981 d after explosion. SN 2011fe exhibits little evolution since the +593 d optical spectrum, but there are several curious aspects in this new extremely late-time regime. We suggest that the persistence of the similar to 5800 angstrom feature is due to NaD, and that a new emission feature at similar to 7300 angstrom may be [Ca II]. Also, we discuss whether the new emission feature at similar to 6400 angstrom might be [Fe I] or the high-velocity hydrogen predicted by Mazzali et al. The nebular feature at 5200 angstrom exhibits linear velocity evolution of similar to 350 km s(-1) per 100 d from at least +220 to +980 d, but the line's shape also changes in this time, suggesting that line blending contributes to the evolution. At similar to 1000 d after explosion, flux from the SN has declined to a point where contribution from a luminous secondary could be detected. In this work, we make the first observational tests for a post-impact remnant star and constrain its temperature and luminosity to T greater than or similar to 10(4) K and L less than or similar to 10(4) L. Additionally, we do not see any evidence for narrow H alpha emission in our spectrum. We conclude that observations continue to strongly exclude many single-degenerate scenarios for SN 2011fe.
C1 [Graham, M. L.; Nugent, P. E.; Filippenko, A. V.; Clubb, K. I.; Zheng, W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Sullivan, M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Cenko, S. B.] 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.
[Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Graham, ML (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM melissalynngraham@gmail.com
OI Sullivan, Mark/0000-0001-9053-4820
FU Google; W. M. Keck Foundation; Gary & Cynthia Bengier; Richard & Rhoda
Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; National
Science Foundation (NSF) [AST-1211916]; Royal Society; NSF Astronomy and
Astrophysics Postdoctoral Fellowship [AST-1302771]
FX Based on observations from the Low Resolution Imaging Spectrometer at
the Keck-1 telescope, the DEep Imaging Multi-Object Spectrograph at the
Keck-2 telescope, and the Kast spectrograph on the 3-m Shane telescope.
We thank the staff at the Lick and Keck Observatories for their
assistance, Ori D. Fox for participating in the observations, and Peter
Lundqvist, Josh Simon, and Ben Shappee for helpful correspondence.
Research at Lick Observatory is partially supported by Google. The W. M.
Keck Observatory is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA; it was made possible by the generous financial support of the W.
M. Keck Foundation. We wish to extend special thanks to those of
Hawaiian ancestry on whose sacred mountain we are privileged to be
guests. The supernova research of AVF's group at U.C. Berkeley is
supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund,
the Christopher R. Redlich Fund, the TABASGO Foundation, and National
Science Foundation (NSF) grant AST-1211916. MS acknowledges support from
the Royal Society. JMS is supported by an NSF Astronomy and Astrophysics
Postdoctoral Fellowship under award AST-1302771.
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SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 1
PY 2015
VL 454
IS 2
BP 1948
EP 1957
DI 10.1093/mnras/stv1888
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA7PZ
UT WOS:000367997700061
ER
PT J
AU Maoz, D
Loeb, A
Shvartzvald, Y
Sitek, M
Engel, M
Kiefer, F
Kiraga, M
Levi, A
Mazeh, T
Pawlak, M
Rich, RM
Tal-Or, L
Wyrzykowski, L
AF Maoz, Dan
Loeb, Abraham
Shvartzvald, Yossi
Sitek, Monika
Engel, Michael
Kiefer, Flavien
Kiraga, Marcin
Levi, Amir
Mazeh, Tsevi
Pawlak, Michal
Rich, R. Michael
Tal-Or, Lev
Wyrzykowski, Lukasz
TI Fast radio bursts: the observational case for a Galactic origin
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars coronae; stars flare; radio continuum: stars
ID SKY AUTOMATED SURVEY; GAMMA-RAY BURSTS; AD-LEONIS; COSMOLOGICAL
DISTANCES; NEUTRON-STARS; FLARES; CONSTRAINTS; DISCOVERY; MERGERS;
SPIKES
AB There are by now ten published detections of fast radio bursts (FRBs) - single bright GHz-band millisecond pulses of unknown origin. Proposed explanations cover a broad range from exotic processes at cosmological distances to atmospheric and terrestrial sources. Loeb, Maoz, and Shvartzvald have previously suggested that FRB sources could be nearby flare stars, and pointed out the presence of a W-UMa-type contact binary within the beam of one out of three FRB fields that they examined. To further test the flare-star hypothesis, we use time-domain optical photometry and spectroscopy, and now find possible flare stars in additional FRB fields, with one to three such cases among all eight FRB fields studied. We evaluate the chance probabilities of these possible associations to be in the range similar to 0.1 per cent to 9 per cent, depending on the input assumptions. Further, we re-analyse the probability that two FRBs recently discovered three years apart within the same radio beam are unrelated. Contrary to other claims, we conclude with 99 per cent confidence that the two events are from the same repeating source. The different dispersion measures between the two bursts then rule out a cosmological intergalactic-medium origin for the dispersion measure, but are consistent with the flare-star scenario with a varying plasma blanket between bursts. Finally, we review some theoretical objections that have been raised against a local flare-star FRB origin, and show that they are incorrect.
C1 [Maoz, Dan; Loeb, Abraham; Shvartzvald, Yossi; Engel, Michael; Kiefer, Flavien; Levi, Amir; Mazeh, Tsevi; Tal-Or, Lev] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Loeb, Abraham] Harvard Univ, Inst Theory & Computat, Cambridge, MA USA.
[Shvartzvald, Yossi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sitek, Monika; Kiraga, Marcin; Pawlak, Michal; Wyrzykowski, Lukasz] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Maoz, D (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
EM maoz@astro.tau.ac.il
FU Sackler Professorship by Special Appointment at Tel Aviv University; NSF
[AST-1312034, AST-1413755]; I-CORE program of the PBC [1829/12]; Israel
Science Foundation; European Research Council under the EU/ERC [291352];
Israel Science Foundation [1423/11]; NASA; University of California;
Polish National Science Center [DEC-2011/03/B/ST9/03299]
FX We thank E. Ofek for his input regarding the localisation of the Lorimer
burst, J. Miralda-Escude for comments, W. Freedman and B. Madore for
data obtained at the Magellan Telescopes, and the anonymous referee for
very useful suggestions. AL acknowledges support from the Sackler
Professorship by Special Appointment at Tel Aviv University. This work
was supported in part by NSF grant AST-1312034 (AL) and Grant 1829/12 of
the I-CORE program of the PBC and the Israel Science Foundation (DM and
TM). The research by TM leading to these results has received funding
from the European Research Council under the EU's Seventh Framework
Programme (FP7/(2007-2013)/ERC Grant Agreement No. 291352), and Israel
Science Foundation grant no. 1423/11 to TM. Research by YS is 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. RMR acknowledges support from NSF grant AST-1413755.
Research at Lick Observatory is supported by the University of
California and partially supported by a generous gift from Google. MK
acknowledges support by the Polish National Science Center under grant
DEC-2011/03/B/ST9/03299.
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SN 0035-8711
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
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EP 2189
DI 10.1093/mnras/stv2105
PG 7
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SC Astronomy & Astrophysics
GA DA7PZ
UT WOS:000367997700078
ER
PT J
AU Lim, JW
AF Lim, J. W.
TI Consideration of structural constraints in passive rotor blade design
for improved performance
SO AERONAUTICAL JOURNAL
LA English
DT Article
ID OPTIMIZATION
AB This design study applied parameterisation to rotor blade for improved performance. In the design, parametric equations were used to represent blade planform changes over the existing rotor blade model. Design variables included blade twist, sweep, dihedral, and radial control point. Updates to the blade structural properties with changes in the design variables allowed accurate evaluation of performance objectives and realistic structural constraints blade stability, steady moments (flap bending, chord bending, and torsion), and the high g manoeuvring pitch link loads. Performance improvement was demonstrated with multiple parametric designs. Using a parametric design with advanced aerofoils, the predicted power reduction was 1-0% in hover, 10.0% at mu = 0.30, and 17.0% at mu = 0.40 relative to the baseline UH-60A rotor, but these were obtained with a 35% increase in the steady chord bending moment at mu = 0.30 and a 20% increase in the half peak-to-peak pitch link load during the UH-60A UTTAS manoeuvre Low vibration was maintained for this design. More rigorous design efforts, such as chord tapering and/or structural redesign of the blade cross section, would enlarge the feasible design space and likely provide significant performance improvement.
C1 [Lim, J. W.] Ames Res Ctr, US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, San Jose, CA 94035 USA.
RP Lim, JW (reprint author), Ames Res Ctr, US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, San Jose, CA 94035 USA.
EM joon.w.lim.civ@mail.mil
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PU ROYAL AERONAUTICAL SOC
PI LONDON
PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND
SN 0001-9240
J9 AERONAUT J
JI Aeronaut. J.
PD DEC
PY 2015
VL 119
IS 1222
BP 1513
EP 1539
PG 27
WC Engineering, Aerospace
SC Engineering
GA DA4JP
UT WOS:000367766500003
ER
PT J
AU Kloog, I
Sorek-Hamer, M
Lyapustin, A
Coull, B
Wang, YJ
Just, AC
Schwartz, J
Broday, DM
AF Kloog, Itai
Sorek-Hamer, Meytar
Lyapustin, Alexei
Coull, Brent
Wang, Yujie
Just, Allan C.
Schwartz, Joel
Broday, David M.
TI Estimating daily PM2.5 and PM10 across the complex geo-climate region of
Israel using MAIAC satellite-based AOD data
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air pollution; Aerosol optical depth (AOD); Epidemiology; PM10; PM2.5;
Exposure error; High particulate levels; MAIAC
ID AEROSOL OPTICAL DEPTH; LAND-USE REGRESSION; PARTICULATE MATTER
PREDICTIONS; NORTHEASTERN USA; ESCAPE PROJECT; MODIS; RETRIEVALS;
PRODUCTS; MODEL; ABSORBENCY
AB Estimates of exposure to PM2.5 are often derived from geographic characteristics based on land-use regression or from a limited number of fixed ground monitors. Remote sensing advances have integrated these approaches with satellite-based measures of aerosol optical depth (AOD), which is spatially and temporally resolved, allowing greater coverage for PM2.5 estimations. Israel is situated in a complex geo-climatic region with contrasting geographic and weather patterns, including both dark and bright surfaces within a relatively small area. Our goal was to examine the use of MODIS-based MAIAC data in Israel, and to explore the reliability of predicted PM2.5 and PM10 at a high spatiotemporal resolution. We applied a three stage process, including a daily calibration method based on a mixed effects model, to predict ground PM2.5 and PM10 over Israel. We later constructed daily predictions across Israel for 2003 2013 using spatial and temporal smoothing, to estimate AOD when satellite data were missing. Good model performance was achieved, with out-of-sample cross validation R-2 values of 0.79 and 0.72 for PM10 and PM2.5, respectively. Model predictions had little bias, with cross-validated slopes (predicted vs. observed) of 0.99 for both the PM2.5 and PM10 models. To our knowledge, this is the first study that utilizes high resolution 1 km MAIAC AOD retrievals for PM prediction while accounting for geo-climate complexities, such as experienced in Israel. This novel model allowed the reconstruction of long- and short-term spatially resolved exposure to PM2.5 and PM10 in Israel, which could be used in the future for epidemiological studies. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Kloog, Itai; Sorek-Hamer, Meytar] Ben Gurion Univ Negev, Dept Geog & Environm Dev, IL-84105 Beer Sheva, Israel.
[Sorek-Hamer, Meytar; Broday, David M.] Technion Israel Inst Technol, Civil & Environm Engn, Haifa, Israel.
[Lyapustin, Alexei] NASA GSFC, Greenbelt, MD USA.
[Coull, Brent] Harvard TH Chan Sch Publ Hlth, Dept Biostat, Boston, MA USA.
[Wang, Yujie] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Just, Allan C.; Schwartz, Joel] Harvard TH Chan Sch Publ Hlth, Dept Environm Hlth, Boston, MA USA.
RP Kloog, I (reprint author), Ben Gurion Univ Negev, Dept Geog & Environm Dev, IL-84105 Beer Sheva, Israel.
EM ikloog@bgu.ac.il
OI Broday, David/0000-0002-6525-3979
FU Environment and Health Fund, Israel
FX We would like to thank the Environment and Health Fund, Israel, for
supporting M.S.H with a doctoral fellowship. The authors would also like
to thank Rakefet Shafran-Natan and Ilan Levy for their help with data
collection.
NR 49
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2015
VL 122
BP 409
EP 416
DI 10.1016/j.atmosenv.2015.10.004
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ9JJ
UT WOS:000367413600042
ER
PT J
AU Behrangi, A
Loikith, PC
Fetzer, EJ
Nguyen, HM
Granger, SL
AF Behrangi, Ali
Loikith, Paul C.
Fetzer, Eric J.
Nguyen, Hai M.
Granger, Stephanie L.
TI Utilizing Humidity and Temperature Data to Advance Monitoring and
Prediction of Meteorological Drought
SO CLIMATE
LA English
DT Article
DE drought; temperature; water vapor; humidity
ID UNITED-STATES; SEASONAL PREDICTION; SOIL-MOISTURE; CLIMATE;
PRECIPITATION; TRENDS; VARIABILITY; SIMULATIONS; FREQUENCY; WEATHER
AB The fraction of land area over the Continental United States experiencing extreme hot and dry conditions has been increasing over the past several decades, consistent with expectation from anthropogenic climate change. A clear concurrent change in precipitation, however, has not been confirmed. Vapor pressure deficit (VPD), combining temperature and humidity, is utilized here as an indicator of the background atmospheric conditions associated with meteorological drought. Furthermore, atmospheric conditions associated with warm season drought events are assessed by partitioning associated VPD anomalies into the temperature and humidity components. This approach suggests that the concurrence of anomalously high temperature and low humidity was an important driver of the rapid development and evolution of the exceptionally severe 2011 Texas and the 2012 Great Plains droughts. By classification of a decade of extreme drought events and tracking them back in time, it was found that near surface atmospheric temperature and humidity add essential information to the commonly used precipitation-based drought indicators and can advance efforts to determine the timing of drought onset and its severity.
C1 [Behrangi, Ali; Fetzer, Eric J.; Nguyen, Hai M.; Granger, Stephanie L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Loikith, Paul C.] Portland State Univ, Dept Geog, Portland, OR 97201 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ali.behrangi@jpl.nasa.gov; ploikith@pdx.edu; Eric.J.Fetzer@jpl.nasa.gov;
Hai.Nguyen@jpl.nasa.gov; Stephanie.L.Granger@jpl.nasa.gov
NR 56
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U1 2
U2 4
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2225-1154
J9 CLIMATE
JI Climate
PD DEC
PY 2015
VL 3
IS 4
BP 999
EP 1017
DI 10.3390/cli3040999
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DA2DQ
UT WOS:000367605900011
ER
PT J
AU Gertych, A
Ing, N
Ma, ZX
Fuchs, TJ
Salman, S
Mohanty, S
Bhele, S
Velasquez-Vacca, A
Amin, MB
Knudsen, BS
AF Gertych, Arkadiusz
Ing, Nathan
Ma, Zhaoxuan
Fuchs, Thomas J.
Salman, Sadri
Mohanty, Sambit
Bhele, Sanica
Velasquez-Vacca, Adriana
Amin, Mahul B.
Knudsen, Beatrice S.
TI Machine learning approaches to analyze histological images of tissues
from radical prostatectomies
SO COMPUTERIZED MEDICAL IMAGING AND GRAPHICS
LA English
DT Article
DE Machine learning; Image analysis; Prostate cancer; Tissue
classification; Tissue quantification
ID PAIRWISE MARKOV-MODELS; INTEROBSERVER REPRODUCIBILITY;
PROSTATIC-CARCINOMA; CANCER; HISTOPATHOLOGY; CLASSIFICATION;
SEGMENTATION; PATHOLOGISTS; GLAND
AB Computerized evaluation of histological preparations of prostate tissues involves identification of tissue components such as stroma (ST), benign/normal epithelium (BN) and prostate cancer (PCa). Image classification approaches have been developed to identify and classify glandular regions in digital images of prostate tissues; however their success has been limited by difficulties in cellular segmentation and tissue heterogeneity. We hypothesized that utilizing image pixels to generate intensity histograms of hematoxylin (H) and eosin (E) stains deconvoluted from H&E images numerically captures the architectural difference between glands and stroma. In addition, we postulated that joint histograms of local binary patterns and local variance (LBPxVAR) can be used as sensitive textural features to differentiate benign/normal tissue from cancer. Here we utilized a machine learning approach comprising of a support vector machine (SVM) followed by a random forest (RF) classifier to digitally stratify prostate tissue into ST, BN and PCa areas. Two pathologists manually annotated 210 images of low- and high-grade tumors from slides that were selected from 20 radical prostatectomies and digitized at high-resolution. The 210 images were split into the training (n = 19) and test (n = 191) sets. Local intensity histograms of H and E were used to train a SVM classifier to separate ST from epithelium (BN+PCa). The performance of SVM prediction was evaluated by measuring the accuracy of delineating epithelial areas. The Jaccard J = 59.5 +/- 14.6 and Rand Ri = 62.0 7.5 indices reported a significantly better prediction when compared to a reference method (Chen et al., Clinical Proteomics 2013, 10:18) based on the averaged values from the test set. To distinguish BN from PCa we trained a RF classifier with LBPxVAR and local intensity histograms and obtained separate performance values for BN and PCa: J(BN) = 35.2 +/- 24.9, O-BN = 49.6 +/- 32, J(PCa) = 49.5 +/- 18.5, O-PCa = 72.7 +/- 14.8 and Ri = 60.6 +/- 7.6 in the test set. Our pixel-based classification does not rely on the detection of lumens, which is prone to errors and has limitations in high-grade cancers and has the potential to aid in clinical studies in which the quantification of tumor content is necessary to prognosticate the course of the disease. The image data set with ground truth annotation is available for public use to stimulate further research in this area. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Gertych, Arkadiusz; Ing, Nathan; Salman, Sadri; Velasquez-Vacca, Adriana] Cedars Sinai Med Ctr, Dept Surg, Los Angeles, CA 90048 USA.
[Gertych, Arkadiusz; Mohanty, Sambit; Bhele, Sanica; Amin, Mahul B.; Knudsen, Beatrice S.] Cedars Sinai Med Ctr, Dept Pathol & Lab Med, Los Angeles, CA 90048 USA.
[Ma, Zhaoxuan; Knudsen, Beatrice S.] Cedars Sinai Med Ctr, Dept Biomed Sci, Los Angeles, CA 90048 USA.
[Fuchs, Thomas J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fuchs, Thomas J.] Mem Sloan Kettering Canc Ctr, Dept Med Phys, New York, NY 10065 USA.
[Fuchs, Thomas J.] Mem Sloan Kettering Canc Ctr, Dept Pathol, New York, NY 10065 USA.
RP Gertych, A (reprint author), Dept Surg, BioImage Informat Lab, 116 N Robertson Blvd,Suite 903, Los Angeles, CA 90048 USA.
EM arkadiusz.gertych@cshs.org
RI Velasquez Vacca, Adriana/L-6787-2013;
OI Velasquez Vacca, Adriana/0000-0002-4867-6371; Gertych,
Arkadiusz/0000-0002-3107-602X
FU Department of Surgery at Cedars-Sinai Medical Center; Department of
Pathology at Cedars-Sinai Medical Center; Department of Biomedical
Sciences at Cedars-Sinai Medical Center; Department of Surgery;
Department of Biomedical Sciences
FX This work was performed in part with the support from the Departments of
Surgery, Pathology and Biomedical Sciences at Cedars-Sinai Medical
Center. Institutional support was provided from the Department of
Surgery to AG and from the Department of Biomedical Sciences to BSK. The
authors would like to thank Elena Chang MD for selecting cases and
marking tumor areas on glass slides before slide digitization and Dr
Yuan Xiaopu for verification of ground truth annotations.
NR 30
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U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0895-6111
EI 1879-0771
J9 COMPUT MED IMAG GRAP
JI Comput. Med. Imaging Graph.
PD DEC
PY 2015
VL 46
SI SI
BP 197
EP 208
DI 10.1016/j.compmedimag.2015.08.002
PN 2
PG 12
WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Radiology, Nuclear Medicine & Medical Imaging
GA DA2NJ
UT WOS:000367632700012
PM 26362074
ER
PT J
AU Evans, JM
Ribeiro, LC
Moore, FB
Wang, SQ
Zhang, QG
Kostas, V
Ferguson, CR
Serrador, J
Falvo, M
Stenger, MB
Goswami, N
Rask, JC
Smith, JD
Knapp, CF
AF Evans, Joyce M.
Ribeiro, L. Christine
Moore, Fritz B.
Wang, Siqi
Zhang, Qingguang
Kostas, Vladimir
Ferguson, Connor R.
Serrador, Jorge
Falvo, Michael
Stenger, Michael B.
Goswami, Nandu
Rask, Jon C.
Smith, Jeffrey D.
Knapp, Charles F.
TI Hypovolemic men and women regulate blood pressure differently following
exposure to artificial gravity
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Orthostatic tolerance; Cardiovascular deconditioning; Centrifugation;
Cardiac output; Stroke volume; Heart rate
ID ORTHOSTATIC TOLERANCE; GENDER-DIFFERENCES; AMBULATORY MEN; SPACEFLIGHT;
HYPOTENSION; EXERCISE; STRESS
AB Purpose In addition to serious bone, vestibular, and muscle deterioration, space flight leads to cardiovascular dysfunction upon return to gravity. In seeking a countermeasure to space flight-induced orthostatic intolerance, we previously determined that exposure to artificial gravity (AG) training in a centrifuge improved orthostatic tolerance of ambulatory subjects. This protocol was more effective in men than women and more effective when subjects exercised.
Methods We now determine the orthostatic tolerance limit (OTL) of cardiovascularly deconditioned (furosemide) men and women on one day following 90 min of AG compared to a control day (90 min of head-down bed rest, HDBR).
Results There were three major findings: a short bout of artificial gravity improved orthostatic tolerance of hypovolemic men (30 %) and women (22 %). Men and women demonstrated different mechanisms of cardiovascular regulation on AG and HDBR days; women maintained systolic blood pressure the same after HDBR and AG exposure while men's systolic pressure dropped (11 +/- 2.9 mmHg) after AG. Third, as presyncopal symptoms developed, men's and women's cardiac output and stroke volume dropped to the same level on both days, even though the OTL test lasted significantly longer on the AG day, indicating cardiac filling as a likely variable to trigger presyncope.
Conclusions (1) Even with gender differences, AG should be considered as a space flight countermeasure to be applied to astronauts before reentry into gravity, (2) men and women regulate blood pressure during an orthostatic stress differently following exposure to artificial gravity and (3) the trigger for presyncope may be cardiac filling.
C1 [Evans, Joyce M.; Wang, Siqi; Zhang, Qingguang; Kostas, Vladimir; Ferguson, Connor R.; Knapp, Charles F.] Univ Kentucky, Dept Biomed Engn, Lexington, KY 40506 USA.
[Ribeiro, L. Christine; Stenger, Michael B.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Moore, Fritz B.; Rask, Jon C.; Smith, Jeffrey D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Serrador, Jorge; Falvo, Michael] Vet Affairs New Jersey Hlth Care Syst, E Orange, NJ USA.
[Goswami, Nandu] Med Univ Graz, Graz, Austria.
RP Evans, JM (reprint author), Univ Kentucky, Dept Biomed Engn, 514G Robot & Mfg Bldg,143 Graham Ave, Lexington, KY 40506 USA.
EM jevans1@uky.edu
OI Zhang, Qingguang/0000-0003-4500-813X; Falvo, Michael/0000-0001-9348-6676
FU KY NASA EPSCoR [NNX07AT58A, KY]; KY State matching Grants; NASA Johnson
Space Center Human Research Program; NASA; War Related Illness & Injury
Study Center, Veterans Administration
FX The authors thank the subjects who volunteered and complied with the
demands of this study. From NASA Ames Research Center, we are grateful
to Dr. Ralph Pelligra for medical monitoring, to Farid Haddad for
centrifuge operation, to Julie Levri for subject recruitment and
scheduling and to Dan Morgan for facilities readiness. From Wyle
Houston, we are grateful to Susan Bourbonais for nursing care and Tim
Caine for heart and blood vessel ultrasound measures. From SUNY
Downstate Medical, we are grateful to Dr Luis Maracaja for analysis of
ultrasound images. From Veterans Affairs New Jersey Health Care System,
we thank Melissa Blatt for subject care. From the University of
Kentucky, we are grateful to Rachel Moore for data collection and
analysis and to Qishan Wu from the Applied Statistical Laboratory for
statistical assistance. This study was supported by KY NASA EPSCoR,
Grant NNX07AT58A, KY; KY State matching Grants; NASA Johnson Space
Center Human Research Program; Supported by NASA and the War Related
Illness & Injury Study Center, Veterans Administration. War Related
Illnesses and Injury Study Center, NJ Veterans Affairs and NASA Ames
Research Center, Division of Space Biosciences and Human Health
Countermeasures Project Element.
NR 17
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U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1439-6319
EI 1439-6327
J9 EUR J APPL PHYSIOL
JI Eur. J. Appl. Physiol.
PD DEC
PY 2015
VL 115
IS 12
BP 2631
EP 2640
DI 10.1007/s00421-015-3261-2
PG 10
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA DA2FN
UT WOS:000367610800015
PM 26438067
ER
PT J
AU Tinetti, G
Drossart, P
Eccleston, P
Hartogh, P
Isaak, K
Linder, M
Lovis, C
Micela, G
Ollivier, M
Puig, L
Ribas, I
Snellen, I
Swinyard, B
Allard, F
Barstow, J
Cho, J
Coustenis, A
Cockell, C
Correia, A
Decin, L
de Kok, R
Deroo, P
Encrenaz, T
Forget, F
Glasse, A
Griffith, C
Guillot, T
Koskinen, T
Lammer, H
Leconte, J
Maxted, P
Mueller-Wodarg, I
Nelson, R
North, C
Palle, E
Pagano, I
Piccioni, G
Pinfield, D
Selsis, F
Sozzetti, A
Stixrude, L
Tennyson, J
Turrini, D
Zapatero-Osorio, M
Beaulieu, JP
Grodent, D
Guedel, M
Luz, D
Norgaard-Nielsen, HU
Ray, T
Rickman, H
Selig, A
Swain, M
Banaszkiewicz, M
Barlow, M
Bowles, N
Branduardi-Raymont, G
du Foresto, VC
Gerard, JC
Gizon, L
Hornstrup, A
Jarchow, C
Kerschbaum, F
Kovacs, G
Lagage, PO
Lim, T
Lopez-Morales, M
Malaguti, G
Pace, E
Pascale, E
Vandenbussche, B
Wright, G
Zapata, GR
Adriani, A
Azzollini, R
Balado, A
Bryson, I
Burston, R
Colome, J
Crook, M
Di Giorgio, A
Griffin, M
Hoogeveen, R
Ottensamer, R
Irshad, R
Middleton, K
Morgante, G
Pinsard, F
Rataj, M
Reess, JM
Savini, G
Schrader, JR
Stamper, R
Winter, B
Abe, L
Abreu, M
Achilleos, N
Ade, P
Adybekian, V
Affer, L
Agnor, C
Agundez, M
Alard, C
Alcala, J
Prieto, CA
Floriano, FJA
Altieri, F
Iglesias, CAA
Amado, P
Andersen, A
Aylward, A
Baffa, C
Bakos, G
Ballerini, P
Banaszkiewicz, M
Barber, RJ
Barrado, D
Barton, EJ
Batista, V
Bellucci, G
Aviles, JAB
Berry, D
Bezard, B
Biondi, D
Blecka, M
Boisse, I
Bonfond, B
Borde, P
Borner, P
Bouy, H
Brown, L
Buchhave, L
Budaj, J
Bulgarelli, A
Burleigh, M
Cabral, A
Capria, MT
Cassan, A
Cavarroc, C
Cecchi-Pestellini, C
Cerulli, R
Chadney, J
Chamberlain, S
Charnoz, S
Jessen, NC
Ciaravella, A
Claret, A
Claudi, R
Coates, A
Cole, R
Collura, A
Cordier, D
Covino, E
Danielski, C
Damasso, M
Deeg, HJ
Delgado-Mena, E
Del Vecchio, C
Demangeon, O
De Sio, A
De Wit, J
Dobrijevic, M
Doel, P
Dominic, C
Dorfi, E
Eales, S
Eiroa, C
Contreras, ME
Esposito, M
Eymet, V
Fabrizio, N
Fernandez, M
Castella, BF
Figueira, P
Filacchione, G
Fletcher, L
Focardi, M
Fossey, S
Fouque, P
Frith, J
Galand, M
Gambicorti, L
Gaulme, P
Lopez, RJG
Garcia-Piquer, A
Gear, W
Gerard, JC
Gesa, L
Giani, E
Gianotti, F
Gillon, M
Giro, E
Giuranna, M
Gomez, H
Gomez-Leal, I
Hernandez, JG
Merino, BG
Graczyk, R
Grassi, D
Guardia, J
Guio, P
Gustin, J
Hargrave, P
Haigh, J
Hebrard, E
Heiter, U
Heredero, RL
Herrero, E
Hersant, F
Heyrovsky, D
Hollis, M
Hubert, B
Hueso, R
Israelian, G
Iro, N
Irwin, P
Jacquemoud, S
Jones, G
Jones, H
Justtanont, K
Kehoe, T
Kerschbaum, F
Kerins, E
Kervella, P
Kipping, D
Koskinen, T
Krupp, N
Lahav, O
Laken, B
Lanza, N
Lellouch, E
Leto, G
Goldaracena, JL
Lithgow-Bertelloni, C
Liu, SJ
Lo Cicero, U
Lodieu, N
Lognonne, P
Lopez-Puertas, M
Lopez-Valverde, MA
Rasmussen, IL
Luntzer, A
Machado, P
MacTavish, C
Maggio, A
Maillard, JP
Magnes, W
Maldonado, J
Mall, U
Marquette, JB
Mauskopf, P
Massi, F
Maurin, AS
Medvedev, A
Michaut, C
Miles-Paez, P
Montalto, M
Rodriguez, PM
Monteiro, M
Montes, D
Morais, H
Morales, JC
Morales-Calderon, M
Morello, G
Martin, AM
Moses, J
Bedon, AM
Alcaino, FM
Oliva, E
Orton, G
Palla, F
Pancrazzi, M
Pantin, E
Parmentier, V
Parviainen, H
Ramirez, KYP
Peralta, J
Perez-Hoyos, S
Petrov, R
Pezzuto, S
Pietrzak, R
Pilat-Lohinger, E
Piskunov, N
Prinja, R
Prisinzano, L
Polichtchouk, I
Poretti, E
Radioti, A
Ramos, AA
Rank-Luftinger, T
Read, P
Readorn, K
Lopez, RR
Rebordao, J
Rengel, M
Rezac, L
Rocchetto, M
Rodler, F
Bejar, VJS
Lavega, AS
Sanroma, E
Santos, N
Forcada, JS
Scandariato, G
Schmider, FX
Scholz, A
Scuderi, S
Sethenadh, J
Shore, S
Showman, A
Sicardy, B
Sitek, P
Smith, A
Soret, L
Sousa, S
Stiepen, A
Stolarski, M
Strazzulla, G
Tabernero, HM
Tanga, P
Tecsa, M
Temple, J
Terenzi, L
Tessenyi, M
Testi, L
Thompson, S
Thrastarson, H
Tingley, BW
Trifoglio, M
Torres, JM
Tozzi, A
Turrini, D
Varley, R
Vakili, F
de Val-Borro, M
Valdivieso, ML
Venot, O
Villaver, E
Vinatier, S
Viti, S
Waldmann, I
Waltham, D
Ward-Thompson, D
Waters, R
Watkins, C
Watson, D
Wawer, P
Wawrzaszk, A
White, G
Widemann, T
Winek, W
Wisniowski, T
Yelle, R
Yung, Y
Yurchenko, SN
AF Tinetti, Giovanna
Drossart, Pierre
Eccleston, Paul
Hartogh, Paul
Isaak, Kate
Linder, Martin
Lovis, Christophe
Micela, Giusi
Ollivier, Marc
Puig, Ludovic
Ribas, Ignasi
Snellen, Ignas
Swinyard, Bruce
Allard, France
Barstow, Joanna
Cho, James
Coustenis, Athena
Cockell, Charles
Correia, Alexandre
Decin, Leen
de Kok, Remco
Deroo, Pieter
Encrenaz, Therese
Forget, Francois
Glasse, Alistair
Griffith, Caitlin
Guillot, Tristan
Koskinen, Tommi
Lammer, Helmut
Leconte, Jeremy
Maxted, Pierre
Mueller-Wodarg, Ingo
Nelson, Richard
North, Chris
Palle, Enric
Pagano, Isabella
Piccioni, Guseppe
Pinfield, David
Selsis, Franck
Sozzetti, Alessandro
Stixrude, Lars
Tennyson, Jonathan
Turrini, Diego
Zapatero-Osorio, Mariarosa
Beaulieu, Jean-Philippe
Grodent, Denis
Guedel, Manuel
Luz, David
Norgaard-Nielsen, Hans Ulrik
Ray, Tom
Rickman, Hans
Selig, Avri
Swain, Mark
Banaszkiewicz, Marek
Barlow, Mike
Bowles, Neil
Branduardi-Raymont, Graziella
du Foresto, Vincent Coude
Gerard, Jean-Claude
Gizon, Laurent
Hornstrup, Allan
Jarchow, Christopher
Kerschbaum, Franz
Kovacs, Geza
Lagage, Pierre-Olivier
Lim, Tanya
Lopez-Morales, Mercedes
Malaguti, Giuseppe
Pace, Emanuele
Pascale, Enzo
Vandenbussche, Bart
Wright, Gillian
Ramos Zapata, Gonzalo
Adriani, Alberto
Azzollini, Ruyman
Balado, Ana
Bryson, Ian
Burston, Raymond
Colome, Josep
Crook, Martin
Di Giorgio, Anna
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Hoogeveen, Ruud
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Pinsard, Frederic
Rataj, Mirek
Reess, Jean-Michel
Savini, Giorgio
Schrader, Jan-Rutger
Stamper, Richard
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Tozzi, A.
Turrini, D.
Varley, R.
Vakili, F.
de Val-Borro, M.
Valdivieso, M. L.
Venot, O.
Villaver, E.
Vinatier, S.
Viti, S.
Waldmann, I.
Waltham, D.
Ward-Thompson, D.
Waters, R.
Watkins, C.
Watson, D.
Wawer, P.
Wawrzaszk, A.
White, G.
Widemann, T.
Winek, W.
Wisniowski, T.
Yelle, R.
Yung, Y.
Yurchenko, S. N.
TI The EChO science case
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Exoplanets; Spectroscopy; Atmospheric science; IR astronomy; Space
missions
ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; EXTRASOLAR PLANET
ATMOSPHERE; INFRARED-EMISSION-SPECTRUM; HOT-JUPITER ATMOSPHERES; GIANT
PLANETS; MU-M; TRANSMISSION SPECTROSCOPY; ENERGY-BALANCE; WATER-VAPOR
AB The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune-all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10(-4) relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 mu m with a goal of covering from 0.4 to 16 mu m. Only modest spectral resolving power is needed, with R similar to 300 for wavelengths less than 5 mu m and R similar to 30 for wavelengths greater than this. The transit spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m(2) is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m(2) telescope, diffraction limited at 3 mu m has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate than current observations. This would enable the detection of molecular abundances three orders of magnitude lower than currently possible and a fourfold increase from the handful of molecules detected to date.
Combining these data with estimates of planetary bulk compositions from accurate measurements of their radii and masses would allow degeneracies associated with planetary interior modelling to be broken, giving unique insight into the interior structure and elemental abundances of these alien worlds. EChO would allow scientists to study exoplanets both as a population and as individuals. The mission can target super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300-3000 K) of F to M-type host stars. The EChO core science would be delivered by a three-tier survey. The EChO Chemical Census: This is a broad survey of a few-hundred exoplanets, which allows us to explore the spectroscopic and chemical diversity of the exoplanet population as a whole. The EChO Origin: This is a deep survey of a subsample of tens of exoplanets for which significantly higher signal to noise and spectral resolution spectra can be obtained to explain the origin of the exoplanet diversity (such as formation mechanisms, chemical processes, atmospheric escape). The EChO Rosetta Stones: This is an ultra-high accuracy survey targeting a subsample of select exoplanets. These will be the bright "benchmark" cases for which a large number of measurements would be taken to explore temporal variations, and to obtain two and three dimensional spatial information on the atmospheric conditions through eclipse-mapping techniques. If EChO were launched today, the exoplanets currently observed are sufficient to provide a large and diverse sample. The Chemical Census survey would consist of > 160 exoplanets with a range of planetary sizes, temperatures, orbital parameters and stellar host properties. Additionally, over the next 10 years, several new ground- and space-based transit photometric surveys and missions will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets.
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RP Tinetti, G (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England.
EM g.tinetti@ucl.ac.uk
RI Sanz-Forcada, Jorge/C-3176-2017; Morales-Calderon, Maria/C-8384-2017;
Coates, Andrew/C-2396-2008; Andersen, Anja Cetti/P-4822-2014; Moses,
Julianne/I-2151-2013; HEBRARD, Eric/E-9257-2014; Montes,
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Lars/C-5625-2012; Michaut, Chloe/F-8561-2010; Rebordao, Jose
Manuel/M-3269-2013; Bouy, Herve/H-2913-2012; Jacquemoud,
Stephane/F-8842-2010; Focardi, Mauro/B-7880-2013; Figueira,
Pedro/J-4916-2013; Barrado Navascues, David/C-1439-2017; Correia,
Alexandre/J-4315-2013; Amado, Pedro Jose/G-3450-2011; Lognonne,
Philippe/F-8846-2010; Morales, Juan Carlos/H-5548-2015; Sanroma,
Esther/L-9273-2015; Guio, Patrick/A-6271-2008; Tennyson,
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Elisa/M-9178-2013; Perez-Hoyos, Santiago/L-7543-2014; Agundez,
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Cetti/0000-0001-8169-7273; Scholz, Aleks/0000-0001-8993-5053; Chadney,
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Sozzetti, Alessandro/0000-0002-7504-365X; Medvedev,
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Michaut, Chloe/0000-0002-2578-0117; Rebordao, Jose
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Navascues, David/0000-0002-5971-9242; Correia,
Alexandre/0000-0002-8946-8579; Amado, Pedro Jose/0000-0002-8388-6040;
Morales, Juan Carlos/0000-0003-0061-518X; Sanroma,
Esther/0000-0001-8859-7937; Guio, Patrick/0000-0002-1607-5862; Tennyson,
Jonathan/0000-0002-4994-5238; Barlow, Michael/0000-0002-3875-1171;
Delgado Mena, Elisa/0000-0003-4434-2195; Perez-Hoyos,
Santiago/0000-0002-2587-4682; Agundez, Marcelino/0000-0003-3248-3564;
Yurchenko, Sergey/0000-0001-9286-9501
FU National Space Agencies
FX We would like to thank all the National Space Agencies who supported the
EChO phase-A study. We also thank Nick Cowan for useful comments.
NR 192
TC 2
Z9 2
U1 5
U2 43
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD DEC
PY 2015
VL 40
IS 2-3
BP 329
EP 391
DI 10.1007/s10686-015-9484-8
PG 63
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA2MC
UT WOS:000367627900002
ER
PT J
AU Varley, R
Waldmann, I
Pascale, E
Tessenyi, M
Hollis, M
Morales, JC
Tinetti, G
Swinyard, B
Deroo, P
Ollivier, M
Micela, G
AF Varley, R.
Waldmann, I.
Pascale, E.
Tessenyi, M.
Hollis, M.
Morales, J. C.
Tinetti, G.
Swinyard, B.
Deroo, P.
Ollivier, M.
Micela, G.
TI Generation of an optimal target list for the exoplanet characterisation
observatory (EChO)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Extrasolar planets; Space mission; Molecular spectroscopy; Transits
ID HUBBLE-SPACE-TELESCOPE; EXTRASOLAR PLANET; TRANSMISSION SPECTROSCOPY; HD
189733B; EMISSION-SPECTRUM; ATMOSPHERIC HAZE; LIGHT-CURVE; GJ 1214B;
DAYSIDE; TRANSIT
AB The Exoplanet Characterisation Observatory (EChO) has been studied as a space mission concept by the European Space Agency in the context of the M3 selection process. Through direct measurement of the atmospheric chemical composition of hundreds of exoplanets, EChO would address fundamental questions such as: What are exoplanets made of? How do planets form and evolve? What is the origin of exoplanet diversity? More specifically, EChO is a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planetary sample within its four to six year mission lifetime. In this paper we use the end-to-end instrument simulator EChOSim to model the currently discovered targets, to gauge which targets are observable and assess the EChO performances obtainable for each observing tier and time. We show that EChO would be capable of observing over 170 relativity diverse planets if it were launched today, and the wealth of optimal targets for EChO expected to be discovered in the next 10 years by space and ground-based facilities is simply overwhelming. In addition, we build on previous molecular detectability studies to show what molecules and abundances will be detectable by EChO for a selection of real targets with various molecular compositions and abundances. EChO's unique contribution to exoplanetary science will be in identifying the main constituents of hundreds of exoplanets in various mass/temperature regimes, meaning that we will be looking no longer at individual cases but at populations. Such a universal view is critical if we truly want to understand the processes of planet formation and evolution in various environments. In this paper we present a selection of key results. The full results are available in Online Resource 1.
C1 [Varley, R.; Waldmann, I.; Tessenyi, M.; Hollis, M.; Tinetti, G.; Swinyard, B.] UCL, London WC1E 6BT, England.
[Pascale, E.] Cardiff Univ, Sch Phys Astron, Cardiff CF24 3AA, S Glam, Wales.
[Morales, J. C.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ollivier, M.] Univ Paris 11, CNRS UMR 8617, IAS, F-91405 Orsay, France.
[Micela, G.] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy.
RP Varley, R (reprint author), UCL, Gower St, London WC1E 6BT, England.
EM r.varley@ucl.ac.uk
RI Morales, Juan Carlos/H-5548-2015;
OI Morales, Juan Carlos/0000-0003-0061-518X; Micela,
Giuseppina/0000-0002-9900-4751; Tinetti, Giovanna/0000-0001-6058-6654
FU UCL IMPACT Studentship; UK Space Agency; STFC; CNES fellowship; ASI/INAF
[I/022/12/0]
FX R. Varley is Funded by a UCL IMPACT Studentship, I. Waldmann is funded
by the UK Space Agency and STFC, J. C. Morales is funded by a CNES
fellowship. G. Tinetti is a Royal Society URF, G. Micela acknowledges
support by the ASI/INAF contract I/022/12/0.
NR 84
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD DEC
PY 2015
VL 40
IS 2-3
BP 621
EP 638
DI 10.1007/s10686-014-9436-8
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DA2MC
UT WOS:000367627900015
ER
PT J
AU Host, NK
Chen, CC
Volakis, JL
Miranda, FA
AF Host, Nicholas K.
Chen, Chi-Chih
Volakis, John L.
Miranda, Felix A.
TI Ku-Band Traveling Wave Slot Array Scanned Via Positioning a Dielectric
Plunger
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Antenna arrays; beam-steering; reconfigurable antenna; satellites; slot
antennas; traveling wave arrays (TWAs)
ID SATELLITE COMMUNICATION; IMPEDANCE SURFACE; BIASED FERRITE; ANTENNA;
BEAM; SUBSTRATE; SYSTEM
AB This paper introduces a feeding concept aimed at eliminating the backend (phase shifters) of traditional phased arrays. A goal is to make phased arrays simpler and less costly for satellite communications. Accordingly, we employ a traveling wave array (TWA) using a single feedline whose propagation constant is controlled via a single, small, and mechanical movement of a dielectric plunger to enable scanning. The dielectric plunger is positioned within a parallel plate waveguide (PPW) transmission line (TL) that feeds the TWA. By adjusting the position of the dielectric plunger within the TL, the feedline achieves a propagation constant range of 1 <= k(eff)/k(0) <= 2.1, corresponding to scan angles of -32.6 degrees <= theta <= 34.2 degrees with an element spacing of d = 0.65 lambda(0). That is, beam steering is achieved using a single feed and a simple linear mechanical movement (for any size array) without using phase shifters. A 20-element array was designed for stable realized gain across -25 degrees <= theta <= 25 degrees beam steering. Additionally, a proof of concept array was fabricated and measured. The simulated copolarized realized gain closely matches the fabricated TWA patterns.
C1 [Host, Nicholas K.; Chen, Chi-Chih; Volakis, John L.] Ohio State Univ, Dept Elect & Comp Engn, Electrosci Lab, Columbus, OH 43212 USA.
[Miranda, Felix A.] NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Host, NK (reprint author), Ohio State Univ, Dept Elect & Comp Engn, Electrosci Lab, Columbus, OH 43212 USA.
EM nhost33@gmail.com
FU National Aeronautics and Space Administration [NNX11AN16H]
FX This work was supported in part by the National Aeronautics and Space
Administration under Grant NNX11AN16H.
NR 33
TC 1
Z9 1
U1 2
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
EI 1558-2221
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD DEC
PY 2015
VL 63
IS 12
BP 5475
EP 5483
DI 10.1109/TAP.2015.2487512
PG 9
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA DA3ZD
UT WOS:000367739000023
ER
PT J
AU Duan, XY
Haynes, M
Moghaddam, M
AF Duan, Xueyang
Haynes, Mark
Moghaddam, Mahta
TI Experimental Verification of the Recursive T-Matrix Method Solutions at
Microwave Frequencies
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Multiple scatterers; random media scattering; recursive T-matrix method
(RTM); scattering measurements
ID SCATTERING-MATRIX; AGGREGATE; ALGORITHM; PARTICLES; SPHERES
AB We present an experimental verification of the recursive T-matrix method (RTM), which is a common method for solving electromagnetic scattering from multiple scatterers. This is done using an antenna and propagation model uniquely suited for T-matrices and network analyzer measurements. In the experiments, we use a multistatic system to measure the scattering from collections of objects consisting of conducting or dielectric spheres, as well as conducting cylinders. In simulation, we calculate the scattering from the objects using the RTM and further predict the transition parameters expected between the receivers and the transmitter in the measurement setup using a propagation model. The predicted andmeasured values of the transmission parameters are compared, and thereby used to verify the recursive T-matrix algorithm. Good agreement observed in these results provides experimental validation of the RTM.
C1 [Duan, Xueyang; Haynes, Mark; Moghaddam, Mahta] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
RP Duan, XY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Xueyang.Duan@jpl.nasa.gov; Mark.S.Haynes@jpl.nasa.gov; mahta@usc.edu
FU National Aeronautics and Space Administration
FX Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 21
TC 0
Z9 0
U1 2
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
EI 1558-2221
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD DEC
PY 2015
VL 63
IS 12
BP 5727
EP 5740
DI 10.1109/TAP.2015.2491967
PG 14
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA DA3ZD
UT WOS:000367739000049
ER
PT J
AU Xapsos, MA
AF Xapsos, Michael A.
TI Conference Comments by the General Chair
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Editorial Material
C1 [Xapsos, Michael A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2375
EP 2377
DI 10.1109/TNS.2015.2502478
PN 1
PG 3
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600001
ER
PT J
AU Dodds, NA
Martinez, MJ
Dodd, PE
Shaneyfelt, MR
Sexton, FW
Black, JD
Lee, DS
Swanson, SE
Bhuva, BL
Warren, KM
Reed, RA
Trippe, J
Sierawski, BD
Weller, RA
Mahatme, N
Gaspard, NJ
Assis, T
Austin, R
Weeden-Wright, SL
Massengill, LW
Swift, G
Wirthlin, M
Cannon, M
Liu, R
Chen, L
Kelly, AT
Marshall, PW
Trinczek, M
Blackmore, EW
Wen, SJ
Wong, R
Narasimham, B
Pellish, JA
Puchner, H
AF Dodds, N. A.
Martinez, M. J.
Dodd, P. E.
Shaneyfelt, M. R.
Sexton, F. W.
Black, J. D.
Lee, D. S.
Swanson, S. E.
Bhuva, B. L.
Warren, K. M.
Reed, R. A.
Trippe, J.
Sierawski, B. D.
Weller, R. A.
Mahatme, N.
Gaspard, N. J.
Assis, T.
Austin, R.
Weeden-Wright, S. L.
Massengill, L. W.
Swift, G.
Wirthlin, M.
Cannon, M.
Liu, R.
Chen, L.
Kelly, A. T.
Marshall, P. W.
Trinczek, M.
Blackmore, E. W.
Wen, S. -J.
Wong, R.
Narasimham, B.
Pellish, J. A.
Puchner, H.
TI The Contribution of Low-Energy Protons to the Total On-Orbit SEU Rate
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Angular effects; error rate prediction; proton direct ionization;
secondary protons; single-event effects (SEEs)
ID SINGLE-EVENT-UPSET; NM SOI SRAM; HARDNESS ASSURANCE; ION ENERGY; IMPACT;
PREDICTIONS; CODE
AB Low- and high-energy proton experimental data and error rate predictions are presented for many bulk Si and SOI circuits from the 20-90 nm technology nodes to quantify how much low-energy protons (LEPs) can contribute to the total on-orbit single-event upset (SEU) rate. Every effort was made to predict LEP error rates that are conservatively high; even secondary protons generated in the spacecraft shielding have been included in the analysis. Across all the environments and circuits investigated, and when operating within 10% of the nominal operating voltage, LEPs were found to increase the total SEU rate to up to 4.3 times as high as it would have been in the absence of LEPs. Therefore, the best approach to account for LEP effects may be to calculate the total error rate from high-energy protons and heavy ions, and then multiply it by a safety margin of 5. If that error rate can be tolerated then our findings suggest that it is justified to waive LEP tests in certain situations. Trends were observed in the LEP angular responses of the circuits tested. Grazing angles were the worst case for the SOI circuits, whereas the worst-case angle was at or near normal incidence for the bulk circuits.
C1 [Dodds, N. A.; Martinez, M. J.; Dodd, P. E.; Shaneyfelt, M. R.; Sexton, F. W.; Black, J. D.; Lee, D. S.; Swanson, S. E.] Sandia Natl Labs, Albuquerque, NM 87123 USA.
[Bhuva, B. L.; Warren, K. M.; Reed, R. A.; Trippe, J.; Sierawski, B. D.; Weller, R. A.; Mahatme, N.; Gaspard, N. J.; Assis, T.; Austin, R.; Weeden-Wright, S. L.; Massengill, L. W.] Vanderbilt Univ, Nashville, TN 37235 USA.
[Swift, G.] Swift Engn & Radiat Serv, San Jose, CA 95124 USA.
[Wirthlin, M.; Cannon, M.] Brigham Young Univ, Provo, UT 84602 USA.
[Liu, R.; Chen, L.] Univ Saskatchewan, Saskatoon, SK S7N 5A2, Canada.
[Kelly, A. T.] BAE Syst, Manassas, VA 20110 USA.
[Marshall, P. W.] US Naval Res Lab, Brookneal, VA 24528 USA.
[Trinczek, M.; Blackmore, E. W.] TRIUMF, Vancouver, BC V6T 2A3, Canada.
[Wen, S. -J.; Wong, R.] Cisco Syst, San Jose, CA 95134 USA.
[Narasimham, B.] Broadcom Corp, Irvine, CA 92617 USA.
[Pellish, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Puchner, H.] Cypress Semicond Inc, San Jose, CA 95134 USA.
RP Dodds, NA (reprint author), Sandia Natl Labs, Albuquerque, NM 87123 USA.
EM nadodds@sandia.gov
FU TRIUMF through the National Research Council of Canada; Laboratory
Directed Research and Development program at Sandia National
Laboratories; U.S. Department of Energy [DE-AC04-94AL85000]
FX This work was supported in part by TRIUMF, which receives funding via a
contribution agreement through the National Research Council of Canada,
and by the Laboratory Directed Research and Development program at
Sandia National Laboratories, a multiprogram laboratory operated by
Sandia Corporation, a Lockheed Martin Company, for the U.S. Department
of Energy, under contract DE-AC04-94AL85000. BAE Systems content
approved for public release under ES-ISR-062515-0457.
NR 34
TC 4
Z9 4
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2440
EP 2451
DI 10.1109/TNS.2015.2486763
PN 1
PG 12
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600011
ER
PT J
AU Adell, PC
Rax, B
Esqueda, IS
Barnaby, HJ
AF Adell, Philippe. C.
Rax, Bernard
Esqueda, Ivan S.
Barnaby, Hugh. J.
TI Hydrogen Limits for Total Dose and Dose Rate Response in Linear Bipolar
Circuits
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Bipolar; ELDRS; hydrogen contamination; packaging; total dose
ID RATE SENSITIVITY ELDRS; RADIATION RESPONSE; MOLECULAR-HYDROGEN;
TRANSISTORS; MECHANISMS; IRRADIATION; DEGRADATION; OXIDES
AB Soaked-hydrogen irradiations show the H-2 limits for the total-dose and dose-rate response of bipolar technologies. We use an analytical model to extrapolate experimental observations and generate an H-2 limits/dose-rate safe-operating-area for various total-dose conditions. Results indicate that 0.1% is the H-2 limit that can impact device degradation. We also show that the impact is larger for higher dose levels and that extra care needs to be taken when qualifying electronics for specific missions.
C1 [Adell, Philippe. C.; Rax, Bernard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Esqueda, Ivan S.] Inst Informat Sci, Marina Del Rey, CA 90292 USA.
[Barnaby, Hugh. J.] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA.
RP Adell, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Philippe.c.adell@jpl.nasa.gov; Ivan.Sanchez@isi.edu; hbarnaby@asu.edu
FU NASA Electronic Part and Packaging program; office of the chief
technologist and scientist at the Jet Propulsion Laboratory
FX This work was supported by the NASA Electronic Part and Packaging
program and the research and development program from the office of the
chief technologist and scientist at the Jet Propulsion Laboratory.
NR 23
TC 1
Z9 1
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2476
EP 2481
DI 10.1109/TNS.2015.2500198
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600015
ER
PT J
AU Casey, MC
Lauenstein, JM
Ladbury, RL
Wilcox, EP
Topper, AD
LaBel, KA
AF Casey, Megan C.
Lauenstein, Jean-Marie
Ladbury, Raymond L.
Wilcox, Edward P.
Topper, Alyson D.
LaBel, Kenneth A.
TI Schottky Diode Derating for Survivability in a Heavy Ion Environment
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Defects; diodes; heavy ion testing; heavy ions; radiation effects in
devices; radiation effects; radiation hardness assurance testing;
radiation hardness assurance; Schottky diodes; semiconductor device
radiation effects; silicon; single-event burnout; single-event charge
collection; single-event effects
ID SINGLE-EVENT BURNOUT; POWER DIODES; RADIATION; SILICON
AB In this paper, we irradiate a number of silicon power Schottky diodes from a variety of manufacturers. The tested diodes represent a wide assortment of reverse voltages and forward currents. Additionally, we review correlations between single-event failures in Schottky diodes and device electrical parameters. The spatial locations of failures in the diode are discussed, as well as a possible explanation for why the failures occur. Based on these correlations to date, we propose a derating scheme for Schottky diodes flown in a heavy ion environment and suggest screening procedures for decreasing the risks of such failures.
C1 [Casey, Megan C.; Lauenstein, Jean-Marie; Ladbury, Raymond L.; LaBel, Kenneth A.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Wilcox, Edward P.; Topper, Alyson D.] AS&D Inc, ASRC Fed Space & Def Inc, Seabrook, MD 20706 USA.
RP Casey, MC (reprint author), NASA, GSFC, Code 561-4, Greenbelt, MD 20771 USA.
EM megan.c.casey@nasa.gov; jean.m.lauenstein@nasa.gov;
raymond.l.ladbury@nasa.gov; ted.wilcox@nasa.gov;
alyson.d.topper@nasa.gov; kenneth.a.label@nasa.gov
FU NASA Electronic Parts and Packaging Program; NEPP; Defense Threat
Reduction Agency (DTRA)
FX This work was supported in part by the NASA Electronic Parts and
Packaging Program, the NEPP, and in part by the Defense Threat Reduction
Agency (DTRA). The work of E. P. Wilcox and A. D. Topper was performed
for the NASA Goddard Space Flight Center (GSFC).
NR 18
TC 1
Z9 1
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2482
EP 2489
DI 10.1109/TNS.2015.2498106
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600016
ER
PT J
AU Wie, BS
LaBel, KA
Turflinger, TL
Wert, JL
Foster, CC
Reed, RA
Kostic, AD
Moss, SC
Guertin, SM
George, JS
Pankuch, M
Dong, L
Bloch, C
Laub, S
AF Wie, Brian S.
LaBel, Kenneth A.
Turflinger, Thomas L.
Wert, Jerry L.
Foster, Charles C.
Reed, Robert A.
Kostic, Andrew D.
Moss, Steven C.
Guertin, Steven M.
George, Jeffrey S.
Pankuch, Mark
Dong, Lei
Bloch, Charles
Laub, Steve
TI Evaluation and Application of US Medical Proton Facilities for Single
Event Effects Test
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Dosimetry; proton beams; radiation hardness assurance; single event
effects
ID HARDNESS ASSURANCE; ENERGY; DOSIMETRY; UPSETS
AB We present the challenges of using new medical proton therapy cyclotrons for SEE tests in the 200 MeV regime. Solutions are discussed to utilize these facilities as a replacement for the Indiana University Cyclotron Facility. Part data response to conventional scattered proton beams are compared to newer scanning beam configurations. A common dosimetry system for independent determination of fluence and beam uniformity is presented.
C1 [Wie, Brian S.] Integr Applicat Inc, Chantilly, VA 20151 USA.
[LaBel, Kenneth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wert, Jerry L.] Boeing Co, Seattle, WA 98018 USA.
[Reed, Robert A.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA.
[Foster, Charles C.] Foster Consulting Serv LLC, University Pl, WA 98466 USA.
[Turflinger, Thomas L.; Kostic, Andrew D.] Aerosp Corp, Chantilly, VA 20151 USA.
[Moss, Steven C.; George, Jeffrey S.] Aerosp Corp, El Segundo, CA 90245 USA.
[Guertin, Steven M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dong, Lei] Scripps Proton Therapy Ctr, San Diego, CA 92121 USA.
[Pankuch, Mark; Laub, Steve] Northwestern Med Chicago Proton Ctr, Warrenville, IL 60555 USA.
[Bloch, Charles] Univ Washington, Dept Radiat Oncol, Seattle, WA 98195 USA.
RP Wie, BS (reprint author), Integr Applicat Inc, Chantilly, VA 20151 USA.
EM bwie@integrity-apps.com
NR 16
TC 0
Z9 0
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2490
EP 2497
DI 10.1109/TNS.2015.2496329
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600017
ER
PT J
AU Ladbury, R
Lauenstein, JM
Hayes, KP
AF Ladbury, R.
Lauenstein, J. -M.
Hayes, K. P.
TI Use of Proton SEE Data as a Proxy for Bounding Heavy-Ion SEE
Susceptibility
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Heavy ions; probabilistic risk assessment; proton radiation effects;
radiation hardness assurance methodology; single-event effect (SEE);
single-event latchup (SEL)
ID SINGLE; MICROELECTRONICS; SPECTRA; LATCHUP; DEVICES; MODEL
AB We examine use of proton single-event effect (SEE) data to constrain heavy-ion SEE susceptibility. We discuss limitations due to short-range proton recoils, especially for destructive SEE modes. We develop an equivalent linear energy transfer metric that reduces risk that proton data will significantly underestimate SEE susceptibility and suggest a probabilistic model for using proton data to constrain device-sensitive volumes.
C1 [Ladbury, R.; Lauenstein, J. -M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hayes, K. P.] Vanderbilt Univ, Nashville, TN 37203 USA.
RP Ladbury, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Raymond.L.Ladbury@nasa.gov; jean.m.lauenstein@nasa.gov;
kathryn.p.hayes@Vanderbilt.edu
NR 20
TC 2
Z9 2
U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2505
EP 2510
DI 10.1109/TNS.2015.2496351
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600019
ER
PT J
AU Quinn, H
Robinson, WH
Rech, P
Aguirre, M
Barnard, A
Desogus, M
Entrena, L
Garcia-Valderas, M
Guertin, SM
Kaeli, D
Kastensmidt, FL
Kiddie, BT
Sanchez-Clemente, A
Reorda, MS
Sterpone, L
Wirthlin, M
AF Quinn, Heather
Robinson, William H.
Rech, Paolo
Aguirre, Miguel
Barnard, Arno
Desogus, Marco
Entrena, Luis
Garcia-Valderas, Mario
Guertin, Steven M.
Kaeli, David
Kastensmidt, Fernanda Lima
Kiddie, Bradley T.
Sanchez-Clemente, Antonio
Reorda, Matteo Sonza
Sterpone, Luca
Wirthlin, Michael
TI Using Benchmarks for Radiation Testing of Microprocessors and FPGAs
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Field-programmable gate arrays (FPGAs); soft error rates; soft errors;
software fault tolerance
ID FAULT-TOLERANCE; SEU; SYSTEMS; DESIGN; LEVEL; CMOS; TOOL
AB Performance benchmarks have been used over the years to compare different systems. These benchmarks can be useful for researchers trying to determine how changes to the technology, architecture, or compiler affect the system's performance. No such standard exists for systems deployed into high radiation environments, making it difficult to assess whether changes in the fabrication process, circuitry, architecture, or software affect reliability or radiation sensitivity. In this paper, we propose a benchmark suite for high-reliability systems that is designed for field-programmable gate arrays and microprocessors. We describe the development process and report neutron test data for the hardware and software benchmarks.
C1 [Quinn, Heather] Los Alamos Natl Lab, ISR Space Data Syst 3, Los Alamos, NM 87545 USA.
[Robinson, William H.; Kiddie, Bradley T.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA.
[Rech, Paolo; Kastensmidt, Fernanda Lima] Univ Fed Rio Grande do Sul, Inst Informat, BR-91501970 Porto Alegre, RS, Brazil.
[Barnard, Arno] Univ Stellenbosch, ZA-7602 Stellenbosch, South Africa.
[Aguirre, Miguel] Univ Seville, Seville 41004, Spain.
[Desogus, Marco; Reorda, Matteo Sonza; Sterpone, Luca] Politecn Torino, I-10129 Turin, TO, Italy.
[Entrena, Luis; Garcia-Valderas, Mario; Sanchez-Clemente, Antonio] Univ Carlos III Madrid, Madrid 28911, Spain.
[Guertin, Steven M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kiddie, Bradley T.] Northeastern Univ, Elect & Comp Engn, Boston, MA 02115 USA.
[Wirthlin, Michael] Brigham Young Univ, Dept Elect & Comp Engn, NSF Ctr High Performance Reconfigurable Comp CHRE, Provo, UT 84602 USA.
RP Quinn, H (reprint author), Los Alamos Natl Lab, ISR Space Data Syst 3, POB 1663, Los Alamos, NM 87545 USA.
EM hquinn@lanl.gov
OI Entrena, Luis/0000-0001-6021-165X
NR 38
TC 4
Z9 4
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2547
EP 2554
DI 10.1109/TNS.2015.2498313
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600025
ER
PT J
AU Chen, DK
Wilcox, E
Berg, M
Kim, H
Phan, A
Figueiredo, M
Seidleck, C
LaBel, K
AF Chen, Dakai
Wilcox, Edward
Berg, Melanie
Kim, Hak
Phan, Anthony
Figueiredo, Marco
Seidleck, Christina
LaBel, Kenneth
TI Single-Event Effect Performance of a Conductive-Bridge Memory EEPROM
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Heavy ion testing; non-volatile memory; radiation effects in ICs;
single-event effect
ID COMMERCIAL NAND
AB We investigated the heavy ion single-event effect (SEE) susceptibility of the industry's first stand-alone memory based on conductive-bridge memory (CBRAM) technology. The device is available as an electrically erasable programmable read-only memory. We found that single-event functional interrupt (SEFI) is the dominant SEE type for each operational mode (standby, dynamic read, and dynamic write/read). SEFIs occurred even while the device is statically biased in standby mode. Worst case SEFIs resulted in errors that filled the entire memory space. Power cycle did not always clear the errors. Thus the corrupted cells had to be reprogrammed in some cases. The device is also vulnerable to bit upsets during dynamic write/read tests, although the frequency of the upsets are relatively low. The linear energy transfer threshold for cell upset is between 10 and MeV . cm(2) / mg, with an upper limit cross section of 1.6 x 10(-11) cm(2) / bit (95% confidence level) at MeV cm mg. In standby mode, the CBRAM array appears invulnerable to bit upsets.
C1 [Chen, Dakai; LaBel, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilcox, Edward; Berg, Melanie; Kim, Hak; Phan, Anthony; Seidleck, Christina] NASA, Goddard Space Flight Ctr, ASRC Space & Def Co, Greenbelt, MD 20771 USA.
[Figueiredo, Marco] NASA, Goddard Space Flight Ctr, Orbital Sci Corp Co, Greenbelt, MD 20771 USA.
RP Chen, DK (reprint author), NASA, Goddard Space Flight Ctr, Code 561, Greenbelt, MD 20771 USA.
EM dakai.chen-1@nasa.gov; ted.wilcox@nasa.gov; marco.a.figueiredo@nasa.gov
FU Adesto Technologies
FX The authors thank Adesto Technologies for technical discussion and
support.
NR 19
TC 0
Z9 0
U1 4
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2703
EP 2708
DI 10.1109/TNS.2015.2476475
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600046
ER
PT J
AU Dodds, NA
Dodd, PE
Shaneyfelt, MR
Sexton, FW
Martinez, MJ
Black, JD
Marshall, PW
Reed, RA
McCurdy, MW
Weller, RA
Pellish, JA
Rodbell, KP
Gordon, MS
AF Dodds, N. A.
Dodd, P. E.
Shaneyfelt, M. R.
Sexton, F. W.
Martinez, M. J.
Black, J. D.
Marshall, P. W.
Reed, R. A.
McCurdy, M. W.
Weller, R. A.
Pellish, J. A.
Rodbell, K. P.
Gordon, M. S.
TI New Insights Gained on Mechanisms of Low-Energy Proton-Induced SEUs by
Minimizing Energy Straggle
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 52nd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 13-17, 2015
CL Boston, MA
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Low-energy protons; proton direct ionization; single-event effects; soft
error rate prediction
ID SINGLE-EVENT-UPSETS; NM SOI SRAM
AB We present low-energy proton single-event upset (SEU) data on a 65 nm SOI SRAM whose substrate has been completely removed. Since the protons only had to penetrate a very thin buried oxide layer, these measurements were affected by far less energy loss, energy straggle, flux attrition, and angular scattering than previous datasets. The minimization of these common sources of experimental interference allows more direct interpretation of the data and deeper insight into SEU mechanisms. The results show a strong angular dependence, demonstrate that energy straggle, flux attrition, and angular scattering affect the measured SEU cross sections, and prove that proton direct ionization is the dominant mechanism for low-energy proton-induced SEUs in these circuits.
C1 [Dodds, N. A.; Dodd, P. E.; Shaneyfelt, M. R.; Sexton, F. W.; Martinez, M. J.; Black, J. D.] Sandia Natl Labs, Albuquerque, NM 87123 USA.
[Marshall, P. W.] NRL Consultant, Brookneal, VA 24528 USA.
[Reed, R. A.; McCurdy, M. W.; Weller, R. A.] Vanderbilt Univ, Nashville, TN 37203 USA.
[Pellish, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rodbell, K. P.; Gordon, M. S.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA.
RP Dodds, NA (reprint author), Sandia Natl Labs, Albuquerque, NM 87123 USA.
EM nadodds@sandia.gov
FU DTRA RHM program
FX The authors would like to thank S. Brown, M. Carts, and A. Boutte for
their assistance with the experiments at NASA Goddard, M. Mendenhall for
his assistance preparing for the experiments at Vanderbilt University,
S. Buchner (Naval Research Laboratory) for his helpful discussions, and
the DTRA RHM program for its support.
NR 21
TC 1
Z9 1
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD DEC
PY 2015
VL 62
IS 6
BP 2822
EP 2829
DI 10.1109/TNS.2015.2488588
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DA3WW
UT WOS:000367732600061
ER
PT J
AU Kim, J
Sanjay, J
Mattmann, C
Boustani, M
Ramarao, MVS
Krishnan, R
Waliser, D
AF Kim, J.
Sanjay, J.
Mattmann, C.
Boustani, M.
Ramarao, M. V. S.
Krishnan, R.
Waliser, D.
TI Uncertainties in estimating spatial and interannual variations in
precipitation climatology in the India-Tibet region from multiple
gridded precipitation datasets
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Article
DE uncertainty; precipitation; observation data; India; regional climate
ID GLOBAL PRECIPITATION; UNITED-STATES; WINTER SEASON; RAIN GAUGES; MODEL;
SIMULATION; VARIABILITY; SENSITIVITY; CALIBRATION; ALGORITHMS
AB Uncertainty in calculating the spatial-and interannual variability of precipitation over India and Tibet from widely used gridded precipitation datasets is examined for the 29-year period from 1979 to 2007. Uncertainty is defined in terms of the spread among the variability calculated from multiple datasets, a useful method when multiple datasets of similar or unknown accuracy are available for analyses. The resulting uncertainty varies for regions and seasons. Geographical variations are clearly seen in the signal-to-noise ratio (SNR), with the largest uncertainty in the Jammu and Kashmir (J&K), western India-eastern Pakistan, Tibet, Hindu-Kush mountains, and Western Ghats which are characterized by either dry climate or complex terrain, or both. Seasonally, the uncertainty is larger for the December-February period (DJF) than for the June-September period (JJAS) in most of the region except J&K which is characterized by two wet seasons: winter and summer. The uncertainty in the interannual variability also varies according to regions especially in J&K where the calculated interannual variability varies by nearly a factor of two among the datasets. The uncertainty range in the calculated interannual variability is determined largely by two gauge-based data of the finest resolution, Asian Precipitation - Highly-Resolved Observational Data Integration Towards Evaluation of water resources (smallest) and India Meteorological Department (largest) in all regions.
The regional and seasonal variations in the uncertainty do not appear to depend on either the spatial resolution or the length of records. This implies that analysis methodology such as the quality control of input data, spatial/temporal interpolation, and retrieval algorithms used in producing these gridded datasets plays a crucial role in determining the characteristics of precipitation climatology represented by individual datasets. Our results show that calculating precipitation characteristics must be accompanied by careful examinations of uncertainty among available datasets, especially for dry seasons and arid/mountainous regions.
C1 [Kim, J.; Waliser, D.] Univ Calif Los Angeles, Atmospher & Ocean Sci, Los Angeles, CA USA.
[Sanjay, J.; Ramarao, M. V. S.; Krishnan, R.] Indian Inst Trop Meteorol, Climate & Global Modelling Div, Pune, Maharashtra, India.
[Mattmann, C.; Boustani, M.; Waliser, D.] CALTECH, Jet Prop Lab, Instrument & Sci Data Syst Sect, Pasadena, CA USA.
RP Kim, J (reprint author), Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90024 USA.
EM jkim@atmos.ucla.edu
FU NASA National Climate Assessment [11-NCA11-0028]; NASA AIST
[AIST-QRS-12-0002]; NSF ExArch [1125798]; Indian Institute of Human
Settlements (IIHS) through the Adaptation at Scale in Semi-Arid Regions
(ASSAR) consortia of the Collaborative Adaptation Research initiative in
Africa and Asia (CARIAA)
FX The contributions by C. Mattmann, M. Boustani, and D. Waliser to this
study were carried out on behalf of the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This research was funded by NASA
National Climate Assessment 11-NCA11-0028, NASA AIST AIST-QRS-12-0002,
and the NSF ExArch 1125798 projects. M. V. S. Ramarao is financially
supported by the Indian Institute of Human Settlements (IIHS) through
the Adaptation at Scale in Semi-Arid Regions (ASSAR) consortia of the
Collaborative Adaptation Research initiative in Africa and Asia
(CARIAA).
NR 41
TC 3
Z9 3
U1 5
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
EI 1097-0088
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD DEC
PY 2015
VL 35
IS 15
BP 4557
EP 4573
DI 10.1002/joc.4306
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DA3XE
UT WOS:000367733700011
ER
PT J
AU Lundgren, P
Kiryukhin, A
Milillo, P
Samsonov, S
AF Lundgren, Paul
Kiryukhin, Alexey
Milillo, Pietro
Samsonov, Sergey
TI Dike model for the 2012-2013 Tolbachik eruption constrained by satellite
radar interferometry observations
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE InSAR; Dike modeling; Tolbachik volcano
ID FORM CROSS-CORRELATION; MAUNA-LOA-VOLCANO; SURFACE DEFORMATION; FISSURE
ERUPTION; CLUSTER-ANALYSIS; KILAUEA VOLCANO; HAWAII; KAMCHATKA;
INVERSION; EARTHQUAKE
AB A large dike intrusion and fissure eruption lasting 9 months began on November 27, 2013, beneath the south flank of Tolbachik Volcano, Kamchatka, Russia. The eruption was the most recent at Tolbachik since the Great Tolbachik Eruption from 1975 to 1976. The 2012 eruption was preceded by more than 6 months of seismicity that clustered beneath the east flank of the volcano along a NW-SE trend. Seismicity increased dramatically before the eruption, with propagation of the seismicity from the central volcano conduit in the final hours. We use interferometric synthetic aperture radar (InSAR) to compute relative displacement images (interferograms) for SAR data pairs spanning the eruption. We use satellite SAR data from the Canadian Space Agency's RADARSAT-2 and from the Italian Space Agency's COSMO-SkyMed missions. Data are modeled first through a Markov Chain Monte Carlo solution for a single tensile dislocation (dike). We then use a boundary element method that includes topography to model a distributed dike-opening model. We find the best-fitting dike dips 80 degrees to the WNW with maximum opening of 6-8 m, localized in the near surface and more broadly distributed in distinct regions up to 3 km beneath the surface, which varies from 1 to 2 km elevation for the eruptive fissures. The distribution of dike opening and its correspondence with co-diking seismicity suggests that the dike propagated radially from Tolbachik's central conduit. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Lundgren, Paul; Milillo, Pietro] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kiryukhin, Alexey] Inst Volcanol & Seismol FEB RAS, Petropavlovsk Kamchatski 683006, Russia.
[Milillo, Pietro] Univ Basilicata, I-85100 Potenza, Italy.
[Samsonov, Sergey] Nat Resources Canada, Canada Ctr Mapping & Earth Observat, Ottawa, ON K1A 0E4, Canada.
RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM paul.lundgren@jpl.nasa.gov
RI Kiryukhin, Alexey/Q-3615-2016;
OI Samsonov, Sergey/0000-0002-6798-4847; Milillo,
Pietro/0000-0002-1171-3976
FU Russia Fund Basic Research [12-05-00125]
FX We thank Dmitry Melnikov for providing digitized lava flow fields for
the 2012-2013 Tolbachik eruption, and facilitated by Ben Edwards. We
thank the Canadian Space Agency for providing RADARSAT-2 data. Part of
this research was carried out using COSMO-SkyMed (CSK (R)) products
delivered under an Italian Space Agency (ASI) license and is made
possible through a collaboration between JPL/Caltech/CIDOT and NASA/ASI.
Fieldwork was supported by Russia Fund Basic Research grant #
12-05-00125. The research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 46
TC 4
Z9 5
U1 4
U2 14
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 DEC 1
PY 2015
VL 307
SI SI
BP 79
EP 88
DI 10.1016/j.jvolgeores.2015.05.011
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DA0NC
UT WOS:000367492900008
ER
PT J
AU Smialek, JL
Garg, A
Gabb, TP
MacKay, RA
AF Smialek, James L.
Garg, Anita
Gabb, Timothy P.
MacKay, Rebecca A.
TI Cyclic Oxidation of High Mo, Reduced Density Superalloys
SO METALS
LA English
DT Article
ID SINGLE-CRYSTAL SUPERALLOYS; CR-AL ALLOYS; BASE SUPERALLOY; SCALE
ADHESION; WATER-VAPOR; RESISTANCE; BEHAVIOR
C1 [Smialek, James L.; Garg, Anita; Gabb, Timothy P.; MacKay, Rebecca A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk, Cleveland, OH 44135 USA.
EM james.l.smialek@nasa.gov; anita.garg-1@nasa.gov;
timothy.p.gabb@nasa.gov; rmackay4462@wowway.com
OI Smialek, James/0000-0003-4310-5569
FU NASA Fundamental Aeronautics Research and Advanced Air Transport
Technology Project Office, Aeronautics Research Mission Directorate
FX This program was initiated and championed by M. Nathal. The XRD analyses
of scale phases by R. Garlick and R. Rogers are gratefully acknowledged.
Funding was provided by the NASA Fundamental Aeronautics Research and
Advanced Air Transport Technology Project Office, Aeronautics Research
Mission Directorate.
NR 30
TC 1
Z9 1
U1 2
U2 7
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2075-4701
J9 METALS-BASEL
JI Metals
PD DEC
PY 2015
VL 5
IS 4
BP 2165
EP 2185
PG 21
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA DA1GU
UT WOS:000367545100028
ER
PT J
AU Zhang, X
West, RA
Irwin, PGJ
Nixon, CA
Yung, YL
AF Zhang, Xi
West, Robert A.
Irwin, Patrick G. J.
Nixon, Conor A.
Yung, Yuk L.
TI Aerosol influence on energy balance of the middle atmosphere of Jupiter
SO NATURE COMMUNICATIONS
LA English
DT Article
ID COLLISION-INDUCED ABSORPTION; JOVIAN AURORAL STRATOSPHERE; INDUCED
INFRARED-SPECTRA; HUBBLE-SPACE-TELESCOPE; H-2-HE PAIRS; TRANSMISSION
SPECTROSCOPY; OPTICAL-CONSTANTS; THERMAL STRUCTURE; GRAVITY-WAVES;
CASSINI CIRS
AB Aerosols are ubiquitous in planetary atmospheres in the Solar System. However, radiative forcing on Jupiter has traditionally been attributed to solar heating and infrared cooling of gaseous constituents only, while the significance of aerosol radiative effects has been a long-standing controversy. Here we show, based on observations from the NASA spacecraft Voyager and Cassini, that gases alone cannot maintain the global energy balance in the middle atmosphere of Jupiter. Instead, a thick aerosol layer consisting of fluffy, fractal aggregate particles produced by photochemistry and auroral chemistry dominates the stratospheric radiative heating at middle and high latitudes, exceeding the local gas heating rate by a factor of 5-10. On a global average, aerosol heating is comparable to the gas contribution and aerosol cooling is more important than previously thought. We argue that fractal aggregate particles may also have a significant role in controlling the atmospheric radiative energy balance on other planets, as on Jupiter.
C1 [Zhang, Xi] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Irwin, Patrick G. J.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England.
[Nixon, Conor A.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Zhang, X (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
EM xiz@ucsc.edu
RI Nixon, Conor/A-8531-2009;
OI Nixon, Conor/0000-0001-9540-9121; Irwin, Patrick/0000-0002-6772-384X
FU Outer Planets Research program via NASA Grant [JPL 1452240]; NASA
Cassini project; UK Science and Technology Facilities Council
FX We thank E. Karkoschka, L. Brown, G. Orton, J. Bailey, T. Kostiuk, A.
Showman and L. Li for useful discussions and comments. Special thanks to
M. Gerstell, P. Gao, R. Hu, P. Kopparla, C. Li, M.C. Liang, S. Newman,
R.L. Shia, M. Wong, X. Xi and Q. Zhang for proofreading the manuscript.
The early phase of this research was supported by the Outer Planets
Research program via NASA Grant JPL 1452240 to the California Institute
of Technology. R.A.W. and C.A.N. are supported by the NASA Cassini
project. P.G.J.I. acknowledges the support of the UK Science and
Technology Facilities Council.
NR 61
TC 1
Z9 1
U1 0
U2 9
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 DEC
PY 2015
VL 6
AR 10231
DI 10.1038/ncomms10231
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DA1SR
UT WOS:000367576300001
PM 26694318
ER
PT J
AU Ali, I
Greifeneder, F
Stamenkovic, J
Neumann, M
Notarnicola, C
AF Ali, Iftikhar
Greifeneder, Felix
Stamenkovic, Jelena
Neumann, Maxim
Notarnicola, Claudia
TI Review of Machine Learning Approaches for Biomass and Soil Moisture
Retrievals from Remote Sensing Data
SO REMOTE SENSING
LA English
DT Review
DE remote sensing; soil moisture; biomass; retrieval algorithms; machine
learning; artificial neural networks; SVM; regression; biophysical
parameters
ID SUPPORT VECTOR MACHINES; LEAF-AREA INDEX; HYPERION HYPERSPECTRAL
IMAGERY; SYNTHETIC-APERTURE RADAR; RADIATIVE-TRANSFER MODEL;
NEURAL-NETWORK APPROACH; POLARIMETRIC SAR DATA; ABOVEGROUND BIOMASS;
FOREST BIOMASS; SATELLITE DATA
AB The enormous increase of remote sensing data from airborne and space-borne platforms, as well as ground measurements has directed the attention of scientists towards new and efficient retrieval methodologies. Of particular importance is the consideration of the large extent and the high dimensionality (spectral, temporal and spatial) of remote sensing data. Moreover, the launch of the Sentinel satellite family will increase the availability of data, especially in the temporal domain, at no cost to the users. To analyze these data and to extract relevant features, such as essential climate variables (ECV), specific methodologies need to be exploited. Among these, greater attention is devoted to machine learning methods due to their flexibility and the capability to process large number of inputs and to handle non-linear problems. The main objective of this paper is to provide a review of research that is being carried out to retrieve two critically important terrestrial biophysical quantities (vegetation biomass and soil moisture) from remote sensing data using machine learning methods.
C1 [Ali, Iftikhar] Natl Univ Ireland Univ Coll Cork, Dept Geog, Cork, Ireland.
[Ali, Iftikhar] TEAGASC, Spatial Anal Unit, Dublin, Ireland.
[Greifeneder, Felix; Notarnicola, Claudia] EURAC Res, Inst Appl Remote Sensing, Bolzano, Italy.
[Stamenkovic, Jelena] Ecole Polytech Fed Lausanne, Signal Proc Lab, CH-1015 Lausanne, Switzerland.
[Neumann, Maxim] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ali, I (reprint author), Natl Univ Ireland Univ Coll Cork, Dept Geog, Cork, Ireland.
EM iftikhar@protonmail.com; felix.greifeneder@eurac.edu;
stamenkovic.jelena@gmail.com; maxim.neumann@jpl.nasa.gov;
claudia.notarnicola@eurac.edu
NR 136
TC 5
Z9 6
U1 27
U2 79
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD DEC
PY 2015
VL 7
IS 12
BP 16398
EP 16421
DI 10.3390/rs71215841
PG 24
WC Remote Sensing
SC Remote Sensing
GA DA1CN
UT WOS:000367534000031
ER
PT J
AU Schroeder, R
McDonald, KC
Chapman, BD
Jensen, K
Podest, E
Tessler, ZD
Bohn, TJ
Zimmermann, R
AF Schroeder, Ronny
McDonald, Kyle C.
Chapman, Bruce D.
Jensen, Katherine
Podest, Erika
Tessler, Zachary D.
Bohn, Theodore J.
Zimmermann, Reiner
TI Development and Evaluation of a Multi-Year Fractional Surface Water Data
Set Derived from Active/Passive Microwave Remote Sensing Data
SO REMOTE SENSING
LA English
DT Article
DE SWAMPS; wetlands; inundation; microwave; backscatter
ID AMAZON RIVER FLOODPLAIN; PROCESS-BASED MODEL; SEASONAL INUNDATION
PATTERNS; COMPARISON PROJECT WETCHIMP; MODERN METHANE EMISSIONS;
SOIL-MOISTURE RETRIEVAL; WIND SCATTEROMETER DATA; NORTHERN
HIGH-LATITUDES; GLOBAL WETLAND EXTENT; NATURAL WETLANDS
AB The sensitivity of Earth's wetlands to observed shifts in global precipitation and temperature patterns and their ability to produce large quantities of methane gas are key global change questions. We present a microwave satellite-based approach for mapping fractional surface water (FW) globally at 25-km resolution. The approach employs a land cover-supported, atmospherically-corrected dynamic mixture model applied to 20+ years (1992-2013) of combined, daily, passive/active microwave remote sensing data. The resulting product, known as Surface WAter Microwave Product Series (SWAMPS), shows strong microwave sensitivity to sub-grid scale open water and inundated wetlands comprising open plant canopies. SWAMPS' FW compares favorably (R-2 = 91%-94%) with higher-resolution, global-scale maps of open water from MODIS and SRTM-MOD44W. Correspondence of SWAMPS with open water and wetland products from satellite SAR in Alaska and the Amazon deteriorates when exposed wetlands or inundated forests captured by the SAR products were added to the open water fraction reflecting SWAMPS' inability to detect water underneath the soil surface or beneath closed forest canopies. Except for a brief period of drying during the first 4 years of observation, the inundation extent for the global domain excluding the coast was largely stable. Regionally, inundation in North America is advancing while inundation is on the retreat in Tropical Africa and North Eurasia. SWAMPS provides a consistent and long-term global record of daily FW dynamics, with documented accuracies suitable for hydrologic assessment and global change-related investigations.
C1 [Schroeder, Ronny; McDonald, Kyle C.; Jensen, Katherine] CUNY City Coll, CUNY Environm CrossRoads Initiat, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Schroeder, Ronny; McDonald, Kyle C.; Jensen, Katherine] CUNY City Coll, NOAA CREST Inst, New York, NY 10031 USA.
[Schroeder, Ronny; Zimmermann, Reiner] Univ Hohenheim, Inst Bot, D-70593 Stuttgart, Germany.
[McDonald, Kyle C.; Chapman, Bruce D.; Podest, Erika] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tessler, Zachary D.] CUNY, Adv Sci Res Ctr, Environm CrossRoads Initiat, New York, NY 10031 USA.
[Bohn, Theodore J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Schroeder, R (reprint author), CUNY City Coll, CUNY Environm CrossRoads Initiat, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
EM ronny.schroder@gmail.com; kmcdonald2@ccny.cuny.edu;
bruce.d.chapman@jpl.nasa.gov; kat.m.jensen@gmail.com;
erika.podest@jpl.nasa.gov; zachary.tessler@asrc.cuny.edu;
theodore.bohn@asu.edu; Dr.Reiner.Zimmermann@uni-hohenheim.de
FU National Science Foundation's Science, Engineering, and Education for
Sustainability program [1216037]; NASA Making Earth Science Data Records
for Use in Research Environments (MEaSUREs) program [NNX11AQ39G]
FX Development of this dataset was supported by the NASA Making Earth
Science Data Records for Use in Research Environments (MEaSUREs) program
funded under contract NNX11AQ39G. The Level 2 SeaWinds-on-QuikSCAT data
were obtained from the Physical Oceanography Distributed Active Archive
Center (PO.DAAC) at the NASA Jet Propulsion Laboratory, Pasadena, CA
(http://podaac.jpl.nasa.gov). Level 2 ASCAT data were acquired from the
NOAA ASCAT near real-time processing system located at the National
Environmental Satellite, Data, and Information Service (NESDIS)
(www.nesdis.noaa.gov). This research was undertaken in part within the
framework of the ALOS Kyoto & Carbon Initiative. The ALOS PALSAR data
were provided by JAXA EORC and the Alaska Satellite Facility (ASF).
Facilities supporting dataset assembly and dissemination have been
provided in part through the NOAA Cooperative Remote Sensing Science and
Technology Center (NOAA-CREST), City College of New York. T. Bohn was
supported by grant 1216037 from the National Science Foundation's
Science, Engineering, and Education for Sustainability program.
NR 140
TC 6
Z9 6
U1 5
U2 17
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD DEC
PY 2015
VL 7
IS 12
BP 16688
EP 16732
DI 10.3390/rs71215843
PG 45
WC Remote Sensing
SC Remote Sensing
GA DA1CN
UT WOS:000367534000046
ER
PT J
AU Reichstetter, M
Fearns, PRCS
Weeks, SJ
McKinna, LIW
Roelfsema, C
Furnas, M
AF Reichstetter, Martina
Fearns, Peter R. C. S.
Weeks, Scarla J.
McKinna, Lachlan I. W.
Roelfsema, Chris
Furnas, Miles
TI Bottom Reflectance in Ocean Color Satellite Remote Sensing for Coral
Reef Environments
SO REMOTE SENSING
LA English
DT Article
DE MODIS; SeaWiFS; optically shallow water; radiative transfer modeling;
spectral separability; cluster analysis
ID GREAT-BARRIER-REEF; SPECTRAL DISCRIMINATION; MACROALGAL COMMUNITIES;
COASTAL ENVIRONMENTS; BENTHIC COMMUNITIES; CLUSTER-ANALYSIS; SHALLOW
WATERS; BATHYMETRY; IMAGERY; MODEL
AB Most ocean color algorithms are designed for optically deep waters, where the seafloor has little or no effect on remote sensing reflectance. This can lead to inaccurate retrievals of inherent optical properties (IOPs) in optically shallow water environments. Here, we investigate in situ hyperspectral bottom reflectance signatures and their separability for coral reef waters, when observed at the spectral resolutions of MODIS and SeaWiFS sensors. We use radiative transfer modeling to calculate the effects of bottom reflectance on the remote sensing reflectance signal, and assess detectability and discrimination of common coral reef bottom classes by clustering modeled remote sensing reflectance signals. We assess 8280 scenarios, including four IOPs, 23 depths and 45 bottom classes at MODIS and SeaWiFS bands. Our results show: (i) no significant contamination (R-rscorr < 0.0005) of bottom reflectance on the spectrally-averaged remote sensing reflectance signal at depths >17 m for MODIS and >19 m for SeaWiFS for the brightest spectral reflectance substrate (light sand) in clear reef waters; and (ii) bottom cover classes can be combined into two distinct groups, light and dark, based on the modeled surface reflectance signals. This study establishes that it is possible to efficiently improve parameterization of bottom reflectance and water-column IOP retrievals in shallow water ocean color models for coral reef environments.
C1 [Reichstetter, Martina; Weeks, Scarla J.; Roelfsema, Chris] Univ Queensland, Sch Geog Planning & Environm Management, Biophys Remote Sensing Res Ctr, St Lucia, Qld 4072, Australia.
[Fearns, Peter R. C. S.] Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, Perth, WA 6845, Australia.
[McKinna, Lachlan I. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McKinna, Lachlan I. W.] Sci Applicat Int Corp, Mclean, VA 22102 USA.
[Furnas, Miles] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
RP Reichstetter, M (reprint author), Univ Queensland, Sch Geog Planning & Environm Management, Biophys Remote Sensing Res Ctr, St Lucia, Qld 4072, Australia.
EM m.reichstetter@uq.edu.au; P.Fearns@curtin.edu.au; s.weeks@uq.edu.au;
lachlan.i.mckinna@nasa.gov; c.roelfsema@uq.edu.au; mjfurnas@gmail.com
FU Australian Research Council Linkage Project Grant [LP100100342]; NASA
Ocean Biology Processing Group; Great Barrier Reef Foundation
FX This research was supported by an Australian Research Council Linkage
Project Grant (LP100100342) with the NASA Ocean Biology Processing Group
and the Great Barrier Reef Foundation. We gratefully acknowledge the
NASA Ocean Biology Processing Group for many helpful discussions. We
thank Bill Venables and Anthony Richardson for their assistance with
designing the statistical approach taken for this study. We thank the
anonymous reviewers for their comments, which have improved the
manuscript.
NR 67
TC 1
Z9 1
U1 3
U2 12
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD DEC
PY 2015
VL 7
IS 12
BP 16756
EP 16777
DI 10.3390/rs71215852
PG 22
WC Remote Sensing
SC Remote Sensing
GA DA1CN
UT WOS:000367534000048
ER
PT J
AU Cougo, MF
Souza, PWM
Silva, AQ
Fernandes, MEB
dos Santos, JR
Abreu, MRS
Nascimento, WR
Simard, M
AF Cougo, Michele F.
Souza-Filho, Pedro W. M.
Silva, Arnaldo Q.
Fernandes, Marcus E. B.
dos Santos, Joao R.
Abreu, Maria R. S.
Nascimento, Wilson R., Jr.
Simard, Marc
TI Radarsat-2 Backscattering for the Modeling of Biophysical Parameters of
Regenerating Mangrove Forests
SO REMOTE SENSING
LA English
DT Article
ID ABOVEGROUND BIOMASS; ELEVATION DATA; ALLOMETRY; CANOPY; COAST;
CLASSIFICATION; MULTIFREQUENCY; ECOSYSTEMS; VEGETATION; HEIGHT
C1 [Cougo, Michele F.; Souza-Filho, Pedro W. M.; Silva, Arnaldo Q.; Abreu, Maria R. S.; Nascimento, Wilson R., Jr.] Fed Univ Para, Inst Geosci, BR-66075110 Belem, Para, Brazil.
[Souza-Filho, Pedro W. M.] Vale Inst Technol, BR-66055090 Belem, Para, Brazil.
[Fernandes, Marcus E. B.] Fed Univ Para, Inst Coastal Studies, Lab Mangrove Ecol, BR-68600000 Braganca, Para, Brazil.
[dos Santos, Joao R.] Natl Inst Space Res INPE, Remote Sensing Dept, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 90039 USA.
RP Souza, PWM (reprint author), Fed Univ Para, Inst Geosci, Cidade Univ,POB 8608, BR-66075110 Belem, Para, Brazil.
EM mcougo@ufpa.br; pedro.martins.souza@itv.org; arnaldoq@ufpa.br;
mebf@ufpa.br; jroberto@dsr.inpe.br; rafaelasalum@ufpa.br;
wilsonrocha81@gmail.com; marc.simard@jpl.nasa.gov
RI Simard, Marc/H-3516-2013; Souza-Filho, Pedro Walfir/J-4958-2012
OI Simard, Marc/0000-0002-9442-4562; Souza-Filho, Pedro
Walfir/0000-0003-0252-808X
FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior
(CAPES-Brazil); Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico (CNPq-Brazil); Universidade Federal do Para and Fundacao de
Amparo e Desenvolvimento da Pesquisa - FADESP; NASA LCLUC program
FX We would like to acknowledge the financial support and field assistance
provided by the Coordenacao de Aperfeicoamento de Pessoal de Nivel
Superior (CAPES-Brazil) and Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico (CNPq-Brazil). We would also like to
acknowledge support provided by Universidade Federal do Para and
Fundacao de Amparo e Desenvolvimento da Pesquisa - FADESP. Thanks are
also extended to the Canadian Spatial Agency, which provided Radarsat-2
images from the "Science and Operational Application Research (SOAR)"
project, and Santiago & Cintra, who provided the RapidEye images. Simard
is supported from the NASA LCLUC program. We would also like to thank
Afonso Quaresma and Edson Pereira for the fieldwork support. Finally, we
would also like to thank the reviewers of this paper and their valuable
contributions towards refining the manuscript.
NR 50
TC 3
Z9 3
U1 4
U2 8
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD DEC
PY 2015
VL 7
IS 12
BP 17097
EP 17112
PG 16
WC Remote Sensing
SC Remote Sensing
GA DA1CS
UT WOS:000367534500008
ER
PT J
AU A, G
Velicogna, I
Kimball, JS
Kim, Y
AF A, G.
Velicogna, I.
Kimball, J. S.
Kim, Y.
TI Impact of changes in GRACE derived terrestrial water storage on
vegetation growth in Eurasia
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE water cycle; terrestrial water storage; satellite remote sensing; GRACE;
ecosystem
ID CANADA BOREAL FORESTS; CLIMATE-CHANGE; FIRE DISTURBANCE; GREENING TREND;
SATELLITE DATA; ARCTIC TUNDRA; DROUGHT; VARIABILITY; SIBERIA; SYSTEM
AB We use GRACE-derived terrestrial water storage (TWS) and ERA-interim air temperature, as proxy for available water and temperature constraints on vegetation productivity, inferred from MODIS satellite normalized difference vegetation index (NDVI), in Northern Eurasia during 2002-2011. We investigate how changes in TWS affect the correlation between NDVI and temperature during the non-frozen season. We find that vegetation growth exhibits significant spatial and temporal variability associated with varying trend in TWS and temperature. The largest NDVI gains occur over boreal forests associated with warming and wetting. The largest NDVI losses occur over grasslands in the Southwestern Ob associated with regional drying and cooling, with dominant constraint from TWS. Over grasslands and temperate forests in the Southeast Ob and South Yenisei, wetting and cooling lead to a dominant temperature constraint due to the relaxation of TWS constraints. Overall, we find significant monthly correlation of NDVI with TWS and temperature over 35% and 50% of the domain, respectively. These results indicate that water availability (TWS) plays a major role in modulating Eurasia vegetation response to temperature changes.
C1 [A, G.; Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kimball, J. S.; Kim, Y.] Univ Montana, Numer Terradynam Simulat Grp, Coll Forestry & Conservat, Missoula, MT 59812 USA.
RP A, G (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM geruoa@uci.edu
FU NASA Cryosphere Program; NASA Terrestrial Hydrology Program; NASA IDS
Program; NASA MEASURES Program; Gordon and Betty Moore Foundation
[GBMF3269]
FX This work was performed at UCI and JPL-Caltech. It was partially
supported by the NASA's Cryosphere, Terrestrial Hydrology, IDS, MEASURES
Programs, Gordon and Betty Moore Foundation (GBMF3269). Data used in
this manuscript are available upon request to the authors. We thank two
anonymous reviewers for their careful reviews.
NR 79
TC 0
Z9 0
U1 6
U2 21
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD DEC
PY 2015
VL 10
IS 12
AR 124024
DI 10.1088/1748-9326/10/12/124024
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ7NO
UT WOS:000367286300031
ER
PT J
AU Kharuk, VI
Ranson, KJ
Im, ST
Petrov, IA
AF Kharuk, Viacheslav I.
Ranson, Kenneth J.
Im, Sergei T.
Petrov, Il'ya A.
TI Climate-induced larch growth response within the central Siberian
permafrost zone
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE larch growth; permafrost thaw; tree ring growth; climate change; water
stress
ID EVERGREEN CONIFERS; GRACE; FOREST; 20TH-CENTURY; TEMPERATURE; TREELINE;
TRENDS; NORTH; SHIFT; USA
AB Aim: estimation of larch (Larix gmelinii) growth response to current climate changes. Location: permafrost area within the northern part of Central Siberia (similar to 65.8 degrees N, 98.5 degrees E). Method: analysis of dendrochronological data, climate variables, drought index SPEI, GPP (gross primary production) and EVI vegetation index (both Aqua/MODIS satellite derived), and soil water content anomalies (GRACE satellite measurements of equivalent water thickness anomalies, EWTA). Results: larch tree ring width (TRW) correlated with previous year August precipitation (r = 0.63), snow accumulation (r = 0.61), soil water anomalies (r = 0.79), early summer temperatures and water vapor pressure (r = 0.73 and r = 0.69, respectively), May and June drought index (r = 0.68-0.82). There are significant positive trends of TRW since late 1980 s and GPP since the year 2000. Mean TRW increased by about 50%, which is similar to post-Little Ice Age warming. TRW correlated with GPP and EVI of larch stands (r = 0.68-0.69). Main conclusions: within the permafrost zone of central Siberia larch TRW growth is limited by early summer temperatures, available water from snowmelt, water accumulated within soil in the previous year, and permafrost thaw water. Water stress is one of the limiting factors of larch growth. Larch TRW growth and GPP increased during recent decades.
C1 [Kharuk, Viacheslav I.; Im, Sergei T.; Petrov, Il'ya A.] Sukachev Inst Forest, Krasnoyarsk, Russia.
[Kharuk, Viacheslav I.; Im, Sergei T.] Siberian Fed Univ, Krasnoyarsk, Russia.
[Im, Sergei T.] Siberian State Aerosp Univ, Krasnoyarsk, Russia.
[Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), Sukachev Inst Forest, Krasnoyarsk, Russia.
EM kharuk@ksc.krasn.ru
RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016
OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938
FU Russian Science Foundation [14-24-00112]; NASA's Terrestrial Ecology
program
FX Authors thanks two anonymous reviewers for helpful comments on a
previous version of the manuscript. Russian Science Foundation (grant
#14-24-00112) supported this research. Additional support for field
measurements by NASA's Terrestrial Ecology program.
NR 51
TC 3
Z9 3
U1 11
U2 33
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD DEC
PY 2015
VL 10
IS 12
AR 125009
DI 10.1088/1748-9326/10/12/125009
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ7NO
UT WOS:000367286300041
ER
PT J
AU Kang, JH
Sauti, G
Park, C
Yamakov, VI
Wise, KE
Lowther, SE
Fay, CC
Thibeault, SA
Bryant, RG
AF Kang, Jin Ho
Sauti, Godfrey
Park, Cheol
Yamakov, Vesselin I.
Wise, Kristopher E.
Lowther, Sharon E.
Fay, Catharine C.
Thibeault, Sheila A.
Bryant, Robert G.
TI Multifunctional Electroactive Nanocomposites Based on Piezoelectric
Boron Nitride Nanotubes
SO ACS NANO
LA English
DT Article
DE boron nitride nanotubes; piezoelectric; electroactive; radiation
shielding; nanocomposite
ID WALL CARBON NANOTUBES; POLYIMIDE; COMPOSITES; RESPONSES; POLYMERS; FILMS
AB Space exploration missions require sensors and devices capable of stable operation in harsh environments such as those that include high thermal fluctuation, atomic oxygen, and high-energy ionizing radiation. However, conventional or state-of-the-art electroactive materials like lead zirconate titanate, poly(vinylidene fluoride), and carbon nanotube (CNT)-doped polyimides have limitations on use in those extreme applications. Theoretical studies have shown that boron nitride nanotubes (BNNTs) have strength-to-weight ratios comparable to those of CNTs, excellent high-temperature stability (to 800 ( in air), large electroactive characteristics, and excellent neutron radiation shielding capability. In this study, we demonstrated the experimental electroactive characteristics of BNNTs in novel multifunctional electroactive nanocomposites. Upon application of an external electric field, the 2 wt % BNNT/polyimide composite was found to exhibit electroactive strain composed of a superposition of linear piezoelectric and nonlinear electrostrictive components. When the BNNTs were aligned by stretching the 2 wt % BNNT/polyimide composite, electroactive characteristics increased by about 460% compared to the nonstretched sample. An all-nanotube actuator consisting of a BNNT buckypaper layer between two single-walled carbon nanotube buckypaper electrode layers was found to have much larger electroactive properties. The additional neutron radiation shielding properties and ultraviolet/visible/near-infrared optical properties of the BNNT composites make them excellent candidates for use in the extreme environments of space missions.
C1 [Kang, Jin Ho; Sauti, Godfrey; Yamakov, Vesselin I.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Park, Cheol; Wise, Kristopher E.; Lowther, Sharon E.; Fay, Catharine C.; Thibeault, Sheila A.; Bryant, Robert G.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Kang, JH (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA.
EM jin.h.kang@nasa.gov; cheol.park-1@nasa.gov
FU NASA Langley Research Center Creativity and Innovation (CI) program;
U.S. Air Force Office of Scientific Research-Low Density Materials
program [FA9550-11-1-0042]
FX This work was supported by the NASA Langley Research Center Creativity
and Innovation (C&I) program. C.P., J.H.K., and G.S. acknowledge that
this work was funded in part by the U.S. Air Force Office of Scientific
Research-Low Density Materials program under Grant No. FA9550-11-1-0042.
C.P. also thanks Dr. W. Cao for HRTEM imaging of BNNTs.
NR 39
TC 7
Z9 8
U1 21
U2 71
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1936-0851
EI 1936-086X
J9 ACS NANO
JI ACS Nano
PD DEC
PY 2015
VL 9
IS 12
BP 11942
EP 11950
DI 10.1021/acsnano.5b04526
PG 9
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA CZ7LE
UT WOS:000367280100043
PM 26529472
ER
PT J
AU Gudmundsson, JE
Ade, PAR
Amiri, M
Benton, SJ
Bock, JJ
Bond, JR
Bryan, SA
Chiang, HC
Contaldi, CR
Crill, BP
Dore, O
Filippini, JP
Fraisse, AA
Gambrel, A
Gandilo, NN
Hasselfield, M
Halpern, M
Hilton, G
Holmes, W
Hristov, VV
Irwin, KD
Jones, WC
Kermish, Z
MacTavish, CJ
Mason, PV
Megerian, K
Moncelsi, L
Montroy, TE
Morford, TA
Nagy, JM
Netterfield, CB
Rahlin, AS
Reintsema, CD
Ruhl, JE
Runyan, MC
Shariff, JA
Soler, JD
Trangsrud, A
Tucker, C
Tucker, RS
Turner, AD
Wiebe, DV
Young, E
AF Gudmundsson, J. E.
Ade, P. A. R.
Amiri, M.
Benton, S. J.
Bock, J. J.
Bond, J. R.
Bryan, S. A.
Chiang, H. C.
Contaldi, C. R.
Crill, B. P.
Dore, O.
Filippini, J. P.
Fraisse, A. A.
Gambrel, A.
Gandilo, N. N.
Hasselfield, M.
Halpern, M.
Hilton, G.
Holmes, W.
Hristov, V. V.
Irwin, K. D.
Jones, W. C.
Kermish, Z.
MacTavish, C. J.
Mason, P. V.
Megerian, K.
Moncelsi, L.
Montroy, T. E.
Morford, T. A.
Nagy, J. M.
Netterfield, C. B.
Rahlin, A. S.
Reintsema, C. D.
Ruhl, J. E.
Runyan, M. C.
Shariff, J. A.
Soler, J. D.
Trangsrud, A.
Tucker, C.
Tucker, R. S.
Turner, A. D.
Wiebe, D. V.
Young, E.
CA SPIDER Collaboration
TI The thermal design, characterization, and performance of the SPIDER
long-duration balloon cryostat
SO CRYOGENICS
LA English
DT Article
DE Instrumentation; Cosmic microwave background; Stratospheric payload;
Cryostat
ID MODE POLARIZATION; REFRIGERATOR
AB We describe the SPIDER flight cryostat, which is designed to cool six millimeter-wavelength telescopes during an Antarctic long-duration balloon flight. The cryostat, one of the largest to have flown on a stratospheric payload, uses liquid He-4 to deliver cooling power to stages at 4.2 and 1.6 K. Stainless steel capillaries facilitate a high flow impedance connection between the main liquid helium tank and a smaller superfluid tank, allowing the latter to operate at 1.6 K as long as there is liquid in the 4.2 K main tank. Each telescope houses a closed cycle He-3 adsorption refrigerator that further cools the focal planes down to 300 mK. Liquid helium vapor from the main tank is routed through heat exchangers that cool radiation shields, providing negative thermal feedback. The system performed successfully during a 17 day flight in the 2014-2015 Antarctic summer. The cryostat had a total hold time of 16.8 days, with 15.9 days occurring during flight. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Gudmundsson, J. E.; Benton, S. J.; Fraisse, A. A.; Gambrel, A.; Jones, W. C.; Kermish, Z.; Rahlin, A. S.; Young, E.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Ade, P. A. R.; Tucker, R. S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Amiri, M.; Hasselfield, M.; Halpern, M.; Wiebe, D. V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Benton, S. J.; Gandilo, N. N.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Montroy, T. E.; Nagy, J. M.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Bock, J. J.; Crill, B. P.; Dore, O.; Holmes, W.; Megerian, K.; Trangsrud, A.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bock, J. J.; Crill, B. P.; Hristov, V. V.; Mason, P. V.; Moncelsi, L.; Morford, T. A.; Runyan, M. C.; Trangsrud, A.; Tucker, R. S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Bond, J. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada.
[Contaldi, C. R.] Imperial Coll, Blackett Lab, Theoret Phys, London, England.
[Reintsema, C. D.] NIST, Boulder, CO USA.
[Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[MacTavish, C. J.] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England.
[Bryan, S. A.] Arizona State Univ, Tempe, AZ USA.
[Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa.
[Shariff, J. A.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Hasselfield, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Soler, J. D.] Inst Astrophys Spatiale, Orsay, France.
[Netterfield, C. B.] Canadian Inst Adv Res CIFAR Program Cosmol Gravit, Toronto, ON, Canada.
RP Gudmundsson, JE (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
FU U.S. by National Aeronautics and Space Administration through the
Science Mission Directorate [NNX07AL64G, NNX12AE95G]; NESSF
[NNX10AM55H]; National Science Foundation [PLR-1043515]; David and
Lucile Packard Foundation; National Sciences and Engineering Council;
Canadian Space Agency
FX SPIDER is supported in the U.S. by National Aeronautics and Space
Administration under Grant No. NNX07AL64G and NNX12AE95G issued through
the Science Mission Directorate, with support for ASR from NESSF
NNX10AM55H, and by the National Science Foundation through PLR-1043515.
Logistical support for the Antarctic deployment and operations was
provided by the NSF through the U.S. Antarctic Program. The
collaboration is grateful for the generous support of the David and
Lucile Packard Foundation, which has been crucial to the success of the
project.; Support in Canada is provided by the National Sciences and
Engineering Council and the Canadian Space Agency.
NR 35
TC 3
Z9 3
U1 2
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0011-2275
EI 1879-2235
J9 CRYOGENICS
JI Cryogenics
PD DEC
PY 2015
VL 72
BP 65
EP 76
DI 10.1016/j.cryogenics.2015.09.002
PN 1
PG 12
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA DA0JG
UT WOS:000367482800009
ER
PT J
AU Dieng, HB
Champollion, N
Cazenave, A
Wada, Y
Schrama, E
Meyssignac, B
AF Dieng, H. B.
Champollion, N.
Cazenave, A.
Wada, Y.
Schrama, E.
Meyssignac, B.
TI Total land water storage change over 2003-2013 estimated from a global
mass budget approach
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE land waters; sea level rise; global water mass budget
ID MEAN SEA-LEVEL; GRACE; RISE
AB We estimate the total land water storage (LWS) change between 2003 and 2013 using a global water mass budget approach. Hereby we compare the ocean mass change (estimated from GRACE space gravimetry on the one hand, and from the satellite altimetry-based global mean sea level corrected for steric effects on the other hand) to the sum of the main water mass components of the climate system: glaciers, Greenland and Antarctica ice sheets, atmospheric water and LWS(the latter being the unknown quantity to be estimated). For glaciers and ice sheets, we use published estimates of ice mass trends based on various types of observations covering different time spans between 2003 and 2013. From the mass budget equation, we derive a net LWS trend over the study period. The mean trend amounts to +0.30 +/- 0.18 mm yr(-1) in sea level equivalent. This corresponds to a net decrease of -108 +/- 64 km 3 yr(-1) in LWS over the 2003-2013 decade. Wealso estimate the rate of change inLWS and find no significant acceleration over the study period. The computed mean global LWS trend over the study period is shown to be explained mainly by direct anthropogenic effects on land hydrology, i.e. the net effect of groundwater depletion and impoundment of water in man-made reservoirs, and to a lesser extent the effect of naturally-forced land hydrology variability. Our results compare well with independent estimates of human-induced changes in global land hydrology.
C1 [Dieng, H. B.; Cazenave, A.; Meyssignac, B.] LEGOS, F-31400 Toulouse, France.
[Champollion, N.; Cazenave, A.] ISSI, CH-3012 Bern, Switzerland.
[Wada, Y.] Univ Utrecht, Dept Phys Geog, NL-3584 CS Utrecht, Netherlands.
[Wada, Y.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Y.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Schrama, E.] Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
RP Dieng, HB (reprint author), LEGOS, 18 Ave E Belin, F-31400 Toulouse, France.
EM habib.dieng@legos.obs-mip.fr
FU ESA (European Space Agency); Japan Society for the Promotion of Science
(JSPS) Oversea Research Fellowship [JSPS-2014-878]
FX H B Dieng is supported by an ESA (European Space Agency) grant in the
context of the Climate Change Initiative (CCI) project. Y Wada is
supported by Japan Society for the Promotion of Science (JSPS) Oversea
Research Fellowship (grant no. JSPS-2014-878). We thank S Yi for
providing us with his GRACE-based land water time series, as well as B
Decharme for making available to us the outputs of the ISBA/TRIP
hydrological model.
NR 32
TC 6
Z9 6
U1 5
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD DEC
PY 2015
VL 10
IS 12
AR 124010
DI 10.1088/1748-9326/10/12/124010
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ7NO
UT WOS:000367286300017
ER
PT J
AU Kharuk, VI
Im, ST
Dvinskaya, ML
Golukov, AS
Ranson, KJ
AF Kharuk, Viacheslav I.
Im, Sergei T.
Dvinskaya, Maria L.
Golukov, Alexei S.
Ranson, Kenneth J.
TI Climate-induced mortality of spruce stands in Belarus
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE conifer mortality; spruce decline; water stress; climate change; drought
stress; tree mortality
ID TREE MORTALITY; NATIONAL-PARK; FOREST; DROUGHT; GROWTH; INFESTATION;
VARIABILITY; ADAPTATION; MOUNTAINS; DYNAMICS
AB The aim of this work is an analysis of the causes of spruce (Picea abies L.) decline and mortality in Belarus. The analysis was based on forest inventory and Landsat satellite (land cover classification, climate variables (air temperature, precipitation, evaporation, vapor pressure deficit, SPEI drought index)), and GRACE-derived soil moisture estimation (equivalent of water thickness anomalies, EWTA). We found a difference in spatial patterns between dead stands and all stands (i.e., before mortality). Dead stands were located preferentially on relief features with higher water stress risk (i.e., higher elevations, steeper slopes, south and southwestern exposure). Spruce mortality followed a series of repeated droughts between 1990 and 2010. Mortality was negatively correlated with air humidity (r = -0.52), and precipitation (r = -0.57), and positively correlated with the prior year vapor pressure deficit (r = 0.47), and drought increase (r = 0.57). Mortality increased with the increase in occurrence of spring frosts (r = 0.5), and decreased with an increase in winter cloud cover (r = -0.37). Spruce mortality was negatively correlated with snow water accumulation (r = -0.81) and previous year anomalies in water soil content (r = -0.8). Weakened by water stress, spruce stands were attacked by pests and phytopathogens. Overall, spruce mortality in Belarussian forests was caused by drought episodes and drought increase in synergy with pest and phytopathogen attacks. Vast Picea abies mortality in Belarus and adjacent areas of Russia and Eastern Europe is a result of low adaptation of that species to increased drought. This indicates the necessity of spruce replacement by drought-tolerant indigenous (e.g., Pinus sylvestris, Querqus robur) or introduced (e.g., Larix sp. or Pseudotsuga menzieslii) species to obtain sustainable forest growth management.
C1 [Kharuk, Viacheslav I.; Im, Sergei T.; Dvinskaya, Maria L.] VN Sukachev Inst Forest SB RAS, Krasnoyarsk, Russia.
[Kharuk, Viacheslav I.; Im, Sergei T.; Golukov, Alexei S.] Siberian Fed Univ, Krasnoyarsk, Russia.
[Im, Sergei T.] Siberian State Aerosp Univ, Krasnoyarsk, Russia.
[Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), VN Sukachev Inst Forest SB RAS, Krasnoyarsk, Russia.
EM kharuk@ksc.krasn.ru
RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016
OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938
FU Russian Science Foundation [14-24-00112]; NASA's Terrestrial Ecology
program
FX The Russian Science Foundation (grant #14-24-00112) primarily supported
this research. Additional support for K J Ranson by NASA's Terrestrial
Ecology program is acknowledged.
NR 54
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U1 5
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD DEC
PY 2015
VL 10
IS 12
AR 125006
DI 10.1088/1748-9326/10/12/125006
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ7NO
UT WOS:000367286300038
ER
PT J
AU Palmer, JG
Cook, ER
Turney, CSM
Allen, K
Fenwick, P
Cook, BI
O'Donnell, A
Lough, J
Grierson, P
Baker, P
AF Palmer, Jonathan G.
Cook, Edward R.
Turney, Chris S. M.
Allen, Kathy
Fenwick, Pavla
Cook, Benjamin I.
O'Donnell, Alison
Lough, Janice
Grierson, Pauline
Baker, Patrick
TI Drought variability in the eastern Australia and New Zealand summer
drought atlas (ANZDA, CE 1500-2012) modulated by the Interdecadal
Pacific Oscillation
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE gridded summer drought atlas; eastern Australia; palaeoclimatology;
Interdecadal Pacific Oscillation (IPO); multi-decadal hydroclimate
variability
ID NORTH-AMERICAN DROUGHT; PALEOCLIMATE RECORDS; LAST MILLENNIUM; CLIMATE;
RAINFALL; TEMPERATURE; RECONSTRUCTIONS; IMPACT; ENSO
AB Agricultural production across eastern Australia and New Zealand is highly vulnerable to drought, but there is a dearth of observational drought information prior to CE 1850. Using a comprehensive network of 176 drought-sensitive tree-ring chronologies and one coral series, we report the first Southern Hemisphere gridded drought atlas extending back to CE 1500. The austral summer (December-February) Palmer drought sensitivity index reconstruction accurately reproduces historically documented drought events associated with the first European settlement of Australia in CE 1788, and the leading principal component explains over 50% of the underlying variance. This leading mode of variability is strongly related to the Interdecadal Pacific Oscillation tripole index (IPO), with a strong and robust antiphase correlation between (1) eastern Australia and the New Zealand North Island and (2) the South Island. Reported positive, negative, and neutral phases of the IPO are consistently reconstructed by the drought atlas although the relationship since CE 1976 appears to have weakened.
C1 [Palmer, Jonathan G.; Turney, Chris S. M.] Univ New S Wales, Sch Biol Earth & Environm Sci, Climate Change Res Ctr, Sydney, NSW 2015, Australia.
[Cook, Edward R.; Cook, Benjamin I.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Allen, Kathy; Baker, Patrick] Univ Melbourne, Sch Ecosyst & Forest Sci, Richmond, Vic 3121, Australia.
[Fenwick, Pavla] Gondwana Tree Ring Lab, Canterbury 7546, New Zealand.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[O'Donnell, Alison; Grierson, Pauline] Univ Western Australia, Sch Plant Biol, Ecosyst Res Grp, Crawley, WA 2016, Australia.
[Lough, Janice] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
RP Palmer, JG (reprint author), Univ New S Wales, Sch Biol Earth & Environm Sci, Climate Change Res Ctr, Sydney, NSW 2015, Australia.
EM j.palmer@unsw.edu.au
RI O'Donnell, Alison/H-8389-2012; Cook, Benjamin/H-2265-2012; Grierson,
Pauline/A-9240-2008;
OI O'Donnell, Alison/0000-0001-7597-7965; Grierson,
Pauline/0000-0003-2135-0272; Turney, Chris/0000-0001-6733-0993; Baker,
Patrick/0000-0002-6560-7124
FU Australian Research Council [FL100100195, LP120100310, DP130104156,
DP0878744, DP120104320, LP120200811, FT120100715]
FX Support was provided by the Australian Research Council through grants:
FL100100195, LP120100310 and DP130104156 for CSMT and DP0878744,
DP120104320, LP120200811, FT120100715 for PJB, Lamont-Doherty Earth
Observatory Contribution No. 7948.
NR 49
TC 12
Z9 12
U1 4
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD DEC
PY 2015
VL 10
IS 12
AR 124002
DI 10.1088/1748-9326/10/12/124002
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ7NO
UT WOS:000367286300009
ER
PT J
AU Munafo, A
Liu, Y
Panesi, M
AF Munafo, A.
Liu, Y.
Panesi, M.
TI Modeling of dissociation and energy transfer in shock-heated nitrogen
flows
SO PHYSICS OF FLUIDS
LA English
DT Article
ID COLLISIONAL-RADIATIVE MODEL; NONEQUILIBRIUM NOZZLE FLOWS;
CHEMICAL-KINETIC PROBLEMS; FUTURE NASA MISSIONS; II FLIGHT EXPERIMENT;
VIBRATIONAL-RELAXATION; THERMOCHEMICAL NONEQUILIBRIUM; HYPERSONIC FLOWS;
AIR; EXCITATION
AB This work addresses the modeling of dissociation and energy transfer processes in shock heated nitrogen flows by means of the maximum entropy linear model and a newly proposed hybrid bin vibrational collisional model. Both models aim at overcoming two of the main limitations of the state of the art non-equilibrium models: (i) the assumption of equilibrium between rotational and translational energy modes of the molecules and (ii) the reliance on the quasi-steady-state distribution for the description of the population of the internal levels. The formulation of the coarse-grained models is based on grouping the energy levels into bins, where the population is assumed to follow a Maxwell-Boltzmann distribution at its own temperature. Different grouping strategies are investigated. Following the maximum entropy principle, the governing equations are obtained by taking the zeroth and first-order moments of the rovibrational master equations. The accuracy of the proposed models is tested against the rovibrational master equation solution for both flow quantities and population distributions. Calculations performed for free-stream velocities ranging from 5 km/s to 10 km/s demonstrate that dissociation can be accurately predicted by using only 2-3 bins. It is also shown that a multi-temperature approach leads to an under-prediction of dissociation, due to the inability of the former to account for the faster excitation of high-lying vibrational states. (C) 2015 AIP Publishing LLC.
C1 [Munafo, A.; Panesi, M.] Univ Illinois, Talbot Lab, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Munafo, A.; Liu, Y.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Munafo, A (reprint author), Univ Illinois, Talbot Lab, Dept Aerosp Engn, 104 S Wright St, Urbana, IL 61801 USA.
EM munafo@illinois.edu; yen.liu@nasa.gov; mpanesi@illinois.edu
OI Liu, Yen/0000-0001-8516-4968
FU Air Force Office of Scientific Research (AFOSR) [FA9550-15-1-0132]; NASA
Entry System Modeling Project in the Space Technology Mission Directory
FX The authors have benefited from numerous discussions with Dr. Richard L.
Jaffe at NASA Ames Research Center. The authors would like to thank Dr.
Alan Wray and Dr. Winifred Huo at NASA Ames Research Center for the
useful suggestions while writing the paper. The research of M.P. and
A.M. is supported by Air Force Office of Scientific Research (AFOSR)
under Young Investigator Program, Grant No. FA9550-15-1-0132. The
research of Yen Liu was sponsored by the NASA Entry System Modeling
Project in the Space Technology Mission Directory. The views and
conclusions contained herein are those of the authors and should not be
interpreted as necessarily representing the official policies or
endorsements, either expressed or implied, of the AFOSR, NASA, or the
U.S. Government.
NR 65
TC 1
Z9 1
U1 2
U2 13
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD DEC
PY 2015
VL 27
IS 12
AR 127101
DI 10.1063/1.4935929
PG 23
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA DA0AO
UT WOS:000367459300037
ER
PT J
AU Rai, RK
Sharma, S
Yadav, N
Goldstein, ML
Sharma, RP
AF Rai, Rajesh Kumar
Sharma, Swati
Yadav, Nitin
Goldstein, M. L.
Sharma, R. P.
TI Effect of magnetic islands on the localization of kinetic Alfven wave
SO PHYSICS OF PLASMAS
LA English
DT Article
ID SOLAR-WIND; RECONNECTION; TURBULENCE; FIELD; MAGNETOTAIL; DYNAMICS;
LINES; SHEET
AB Recent studies have revealed an intimate link between magnetic reconnection and turbulence. Observations show that kinetic Alfven waves (KAWs) play a very crucial role in magnetic reconnection and have been a topic of interest from decades in the context of turbulence and particle heating. In the present paper, we study the role that KAW plays in the formation of coherent structures/ current sheets when KAW is propagating in the pre-existing fully developed chain of magnetic islands. We derived the dynamical equation of KAW in the presence of chain of magnetic islands and solved it using numerical simulations well as analytic tools. Due to pre- existing chain of magnetic islands, KAW splits into coherent structures and the scale size of these structures along transverse directions (with respect to background magnetic field) comes out to be either less than or greater than ion gyro radius. Therefore, the present work may be the first step towards understanding how magnetic reconnection generated islands may affect the KAW localization and eventually contribute to magnetic turbulence. In this way the present approach may be helpful to understand the interplay between magnetic reconnection and turbulence in ion diffusion region. (C) 2015 AIP Publishing LLC.
C1 [Rai, Rajesh Kumar; Sharma, Swati; Yadav, Nitin; Sharma, R. P.] Indian Inst Technol Delhi, Ctr Energy Studies, New Delhi 110016, India.
[Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rai, RK (reprint author), Indian Inst Technol Delhi, Ctr Energy Studies, New Delhi 110016, India.
EM rajanraj.rai7@gmail.com; swati.sharma704@gmail.com
RI NASA MMS, Science Team/J-5393-2013;
OI NASA MMS, Science Team/0000-0002-9504-5214; GOLDSTEIN,
MELVYN/0000-0002-5317-988X
FU Council for Scientific and Industrial Research (CSIR) [221251160];
Indian Space Research Organization (ISRO) under RESPOND Program;
Department of Science and Technology (DST), India
FX We acknowledge fruitful and helpful discussions by Paul Cassak. This
work was partially supported by the Council for Scientific and
Industrial Research (CSIR) under Grant No. 221251160, Indian Space
Research Organization (ISRO) under RESPOND Program and the Department of
Science and Technology (DST), India.
NR 32
TC 2
Z9 2
U1 1
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD DEC
PY 2015
VL 22
IS 12
AR 122106
DI 10.1063/1.4936873
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA DA0AZ
UT WOS:000367460400016
ER
PT J
AU Li, JR
Flagg, C
Okin, GS
Painter, TH
Dintwe, K
Belnap, J
AF Li, Junran
Flagg, Cody
Okin, Gregory S.
Painter, Thomas H.
Dintwe, Kebonye
Belnap, Jayne
TI On the prediction of threshold friction velocity of wind erosion using
soil reflectance spectroscopy
SO AEOLIAN RESEARCH
LA English
DT Article
DE Dust; Wind erosion; Remote sensing; Partial least squares regression
ID ATMOSPHERIC DUST CYCLE; GRAIN-SIZE; SPECTRAL CHARACTERISTICS; SEMIARID
ENVIRONMENTS; MODEL; CRUST; DISTURBANCE; VEGETATION; EMISSION; DESERT
AB Current approaches to estimate threshold friction velocity (TFV) of soil particle movement, including both experimental and empirical methods, suffer from various disadvantages, and they are particularly not effective to estimate TFVs at regional to global scales. Reflectance spectroscopy has been widely used to obtain TFV-related soil properties (e.g., moisture, texture, crust, etc.), however, no studies have attempted to directly relate soil TFV to their spectral reflectance. The objective of this study was to investigate the relationship between soil TFV and soil reflectance in the visible and near infrared (VIS-NIR, 350-2500 nm) spectral region, and to identify the best range of wavelengths or combinations of wavelengths to predict TFV. Threshold friction velocity of 31 soils, along with their reflectance spectra and texture were measured in the Mojave Desert, California and Moab, Utah. A correlation analysis between TFV and soil reflectance identified a number of isolated, narrow spectral domains that largely fell into two spectral regions, the VIS area (400-700 nm) and the short-wavelength infrared (SWIR) area (1100-2500 nm). A partial least squares regression analysis (PLSR) confirmed the significant bands that were identified by correlation analysis. The PLSR further identified the strong relationship between the first-difference transformation and TFV at several narrow regions around 1400,1900, and 2200 nm. The use of PLSR allowed us to identify a total of 17 key wavelengths in the investigated spectrum range, which may be used as the optimal spectral settings for estimating TFV in the laboratory and field, or mapping of TFV using airborne/satellite sensors. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Li, Junran] Univ Tulsa, Dept Geosci, Tulsa, OK 74104 USA.
[Flagg, Cody] Natl Ecol Observ Network, Boulder, CO 80301 USA.
[Okin, Gregory S.; Dintwe, Kebonye] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Painter, Thomas H.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Belnap, Jayne] US Geol Survey, Southwest Biol Sci Ctr, Moab, UT 84532 USA.
RP Li, JR (reprint author), Univ Tulsa, Dept Geosci, Tulsa, OK 74104 USA.
EM junran@utulsa.edu
RI Painter, Thomas/B-7806-2016
FU NASA [NNX10AO97G]; NSF [EAR-1148334]; Department of Transportation
Southern Plains Transportation Center [SPTC14.1-39]; U.S. Geological
Survey Ecosystems and Climate and Land Use programs; National
Aeronautics and Space Administration
FX This research was supported by NASA Grant NNX10AO97G, NSF Grant
EAR-1148334, and Department of Transportation Southern Plains
Transportation Center Grant SPTC14.1-39. JB was supported by the U.S.
Geological Survey Ecosystems and Climate and Land Use programs. Part of
this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology under a contract with the National Aeronautics
and Space Administration. Any use of trade names is for descriptive
purposes only and does not imply endorsement by the U.S. Government.
NR 30
TC 1
Z9 1
U1 3
U2 12
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1875-9637
EI 2212-1684
J9 AEOLIAN RES
JI Aeolian Res.
PD DEC
PY 2015
VL 19
BP 129
EP 136
DI 10.1016/j.aeolia.2015.10.001
PN A
PG 8
WC Geography, Physical
SC Physical Geography
GA CZ3RY
UT WOS:000367022900011
ER
PT J
AU Barucci, MA
Ore, CMD
Perna, D
Cruikshank, DP
Doressoundiram, A
Alvarez-Candal, A
Dotto, E
Nitschelm, C
AF Barucci, M. A.
Ore, C. M. Dalle
Perna, D.
Cruikshank, D. P.
Doressoundiram, A.
Alvarez-Candal, A.
Dotto, E.
Nitschelm, C.
TI (50000) Quaoar: Surface composition variability
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Kuiper belt objects: individual: (50000) Quaoar; techniques:
spectroscopic
ID TRANS-NEPTUNIAN OBJECTS; CRYSTALLINE WATER ICE; ESO LARGE PROGRAM;
KUIPER-BELT; MU-M; OPTICAL-PROPERTIES; ION IRRADIATION; X-SHOOTER;
CENTAURS; METHANE
AB Aims. The goal of this work is to investigate the composition of the surface of (50000) Quaoar and its spatial variability.
Methods. We present new continuous spectra from the visible to near-IR (0.3-2.3 mu m) obtained with the X-Shooter instrument at the VLT-ESO at four different epochs on the surface of Quaoar. The data represent the highest spectral resolution data ever obtained for this object and the first near-IR dataset acquired in a single exposure over the entire wavelength range. They are complemented by previously published photometric observations obtained in the near-IR (3.6, 4.5 mu m) with the Spitzer Space Telescope, which provide an extra set of constraints in the model calculation. Spectral modelling was performed for the entire wavelength range by means of a code based on the Shkuratov radiative transfer formulation and of an updated value of albedo obtained from recent Herschel observations.
Results. We obtained compositional information for different observed areas that can cover about 40% of the assumed rotational period of 8.84 h. Our analysis helps to prove the presence of CH4 and C2H6, as previously reported, along with indications of the possible presence of NH3 center dot H2O. New evidence of N-2 is inferred from the shift in the CH4 bands. The albedo at the two Spitzer bands suggests there may be CO diluted in N-2, and CO2 for one of the surface locations.
Conclusions. The spectral similarities indicate the overall homogeneity of the surface composition of one hemisphere of Quaoar, while some subtle variations are apparent when modelling. The presence of NH3 center dot H2O would support the idea that Quaoar's surface may be relatively young.
C1 [Barucci, M. A.; Perna, D.; Doressoundiram, A.] Univ Paris 06, Univ Paris Diderot, Sorbonne Paris Cite, PSL Res Univ,Sorbonne Univ,Observ Paris,CNRS,LESI, F-92195 Meudon, France.
[Ore, C. M. Dalle; Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Alvarez-Candal, A.] Observ Nacl, Rio De Janeiro, Brazil.
[Dotto, E.] Osserv Astron Roma, INAF, I-00040 Rome, Italy.
[Nitschelm, C.] Univ Antofagasta, Fac Ciencias Bas, Unidad Astron, Antofagasta, Chile.
[Ore, C. M. Dalle] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
RP Barucci, MA (reprint author), Univ Paris 06, Univ Paris Diderot, Sorbonne Paris Cite, PSL Res Univ,Sorbonne Univ,Observ Paris,CNRS,LESI, F-92195 Meudon, France.
EM antonella.barucci@obspm.fr
RI Alvarez-Candal, Alvaro/M-4834-2013;
OI Dotto, Elisabetta/0000-0002-9335-1656
FU European Southern Observatory (ESO), Chile [091.C-0057]; French
Planetology National Programme (INSU-PNP); Outer Planets Research grant
NASA [NNX12AM75G]; CNPq; FAPERJ
FX Based on observations carried out at the European Southern Observatory
(ESO), Chile (programme 091.C-0057). The project is supported by the
French Planetology National Programme (INSU-PNP). C.M.D.O. acknowledges
support from the Outer Planets Research grant NASA NNX12AM75G. A.A.C.
acknowledges financial support from CNPq and FAPERJ through diverse
grants.
NR 49
TC 0
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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 DEC
PY 2015
VL 584
AR A107
DI 10.1051/0004-6361/201526119
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800107
ER
PT J
AU Britavskiy, NE
Bonanos, AZ
Mehner, A
Boyer, ML
McQuinn, KBW
AF Britavskiy, N. E.
Bonanos, A. Z.
Mehner, A.
Boyer, M. L.
McQuinn, K. B. W.
TI Identification of dusty massive stars in star-forming dwarf irregular
galaxies in the Local Group with mid-IR photometry
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: massive; stars: late-type; galaxies: individual: Sex A;
supergiants
ID LUMINOUS BLUE VARIABLES; INFRARED CAII TRIPLET; WOLF-LUNDMARK-MELOTTE;
RED SUPERGIANT STARS; EMISSION-LINE STARS; NEARBY GALAXIES; MAGELLANIC
CLOUDS; EMPIRICAL CALIBRATION; UBVRI PHOTOMETRY; STELLAR CONTENT
AB Context. Increasing the statistics of spectroscopically confirmed evolved massive stars in the Local Group enables the investigation of the mass loss phenomena that occur in these stars in the late stages of their evolution.
Aims. We aim to complete the census of luminous mid-IR sources in star-forming dwarf irregular (dIrr) galaxies of the Local Group. To achieve this we employed mid-IR photometric selection criteria to identify evolved massive stars, such as red supergiants (RSGs) and luminous blue variables (LBVs), by using the fact that these types of stars have infrared excess due to dust.
Methods. The method is based on 3.6 mu m and 4.5 mu m photometry from archival Spitzer Space Telescope images of nearby galaxies. We applied our criteria to four dIrr galaxies: Pegasus, Phoenix, Sextans A, and WLM, selecting 79 point sources that we observed with the VLT/FORS2 spectrograph in multi-object spectroscopy mode.
Results. We identified 13 RSGs, of which 6 are new discoveries, as well as two new emission line stars, and one candidate yellow supergiant. Among the other observed objects we identified carbon stars, foreground giants, and background objects, such as a quasar and an early-type galaxy that contaminate our survey. We use the results of our spectroscopic survey to revise the mid-IR and optical selection criteria for identifying RSGs from photometric measurements. The optical selection criteria are more efficient in separating extragalactic RSGs from foreground giants than mid-IR selection criteria, but the mid-IR selection criteria are useful for identifying dusty stars in the Local Group. This work serves as a basis for further investigation of the newly discovered dusty massive stars and their host galaxies.
C1 [Britavskiy, N. E.; Bonanos, A. Z.] Natl Observ Athens, IAASARS, Penteli 15236, Greece.
[Britavskiy, N. E.] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, Athens 15783, Greece.
[Mehner, A.] ESO European Org Astron Res Southern Hemisphere, Santiago, Chile.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[McQuinn, K. B. W.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
RP Britavskiy, NE (reprint author), Natl Observ Athens, IAASARS, Penteli 15236, Greece.
EM britavskiy@astro.noa.gr; bonanos@astro.noa.gr
RI Bonanos, Alceste/K-5392-2013
OI Bonanos, Alceste/0000-0003-2851-1905
FU European Union (European Social Fund); National Resources under the
"ARISTEIA" action of the Operational Programme "Education and Lifelong
Learning" in Greece; Alfred P. Sloan Foundation; National Science
Foundation; US Department of Energy Office of Science
FX We thank the anonymous referee for helpful comments that have improved
the manuscript. N. Britavskiy and A.Z. Bonanos acknowledge funding by
the European Union (European Social Fund) and National Resources under
the "ARISTEIA" action of the Operational Programme "Education and
Lifelong Learning" in Greece. We would like to thank A. Miroshnichenko
for useful discussions on the identification of emission lines in
spectra. This research has made use of NASA's Astrophysics Data System
Bibliographic Services and the VizieR catalogue access tool, CDS,
Strasbourg, France. 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.
NR 57
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U2 2
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 DEC
PY 2015
VL 584
AR A33
DI 10.1051/0004-6361/201526393
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800033
ER
PT J
AU Huby, E
Baudoz, P
Mawet, D
Absil, O
AF Huby, E.
Baudoz, P.
Mawet, D.
Absil, O.
TI Post-coronagraphic tip-tilt sensing for vortex phase masks: The QACITS
technique
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: high angular resolution; methods: analytical; methods:
numerical
ID LABORATORY DEMONSTRATION; COMPANION; BEAMWIDTHS; CANDIDATE; PRINCIPLE;
DISCOVERY; VLT/NACO; IMAGES; SENSOR; STAR
AB Context. Small inner working angle coronagraphs, such as the vortex phase mask, are essential to exploit the full potential of ground-based telescopes in the context of exoplanet detection and characterization. However, the drawback of this attractive feature is a high sensitivity to pointing errors, which degrades the performance of the coronagraph.
Aims. We propose a tip-tilt retrieval technique based on the analysis of the final coronagraphic image, hereafter called Quadrant Analysis of Coronagraphic Images for Tip-tilt Sensing (QACITS).
Methods. Under the assumption of small phase aberrations, we show that the behavior of the vortex phase mask can be simply described from the entrance pupil to the Lyot stop plane with Zernike polynomials. This convenient formalism is used to establish the theoretical basis of the QACITS technique. We performed simulations to demonstrate the validity and limits of the technique, including the case of a centrally obstructed pupil.
Results. The QACITS technique principle is validated with experimental results in the case of an unobstructed circular aperture, as well as simulations in presence of a central obstruction. The typical configuration of the Keck telescope (24% central obstruction) has been simulated with additional high order aberrations. In these conditions, our simulations show that the QACITS technique is still adapted to centrally obstructed pupils and performs tip-tilt retrieval with a precision of 5 x 10(-2) lambda/D when wavefront errors amount to lambda/14 rms and 10(-2) lambda/D for lambda/70 rms errors (with lambda the wavelength and D the pupil diameter).
Conclusions. We have developed and demonstrated a tip-tilt sensing technique for vortex coronagraphs. The implementation of the QACITS technique is based on the analysis of the scientific image and does not require any modification of the original setup. Current facilities equipped with a vortex phase mask can thus directly benefit from this technique to improve the contrast performance close to the axis.
C1 [Huby, E.; Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
[Baudoz, P.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris,Paris Sci & Lettres, F-92195 Meudon, France.
[Mawet, D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Mawet, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Huby, E (reprint author), Univ Liege, Dept Astrophys Geophys & Oceanog, 19 Allee Six Aout, B-4000 Liege, Belgium.
EM elsa.huby@ulg.ac.be
FU European Research Council under the European Union [337569]; French
Community of Belgium through ARC
FX The research leading to these results has received funding from the
European Research Council under the European Union's Seventh Framework
Programme (ERC Grant Agreement n. 337569) and from the French Community
of Belgium through an ARC grant for Concerted Research Action.
NR 31
TC 5
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U1 0
U2 2
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 DEC
PY 2015
VL 584
AR A74
DI 10.1051/0004-6361/201527102
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800074
ER
PT J
AU Jeffrey, NLS
Kontar, EP
Dennis, BR
AF Jeffrey, Natasha L. S.
Kontar, Eduard P.
Dennis, Brian R.
TI High-temperature differential emission measure and altitude variations
in the temperature and density of solar flare coronal X-ray sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: flares; Sun: corona; Sun: X-rays, gamma rays; Sun: particle
emission
ID ELECTRON ACCELERATION; MAGNETIC RECONNECTION; ATOMIC DATABASE; RHESSI;
LOOP; FIELD; SPECTRA; REGIONS; CHIANTI; ENERGY
AB The detailed knowledge of plasma heating and acceleration region properties presents a major observational challenge in solar flare physics. Using the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the high temperature differential emission measure, DEM(T), and the energy-dependent spatial structure of solar flare coronal sources were studied quantitatively. The altitude of the coronal X-ray source was observed to increase with energy by similar to+0.2 arcsec/keV between 10 and 25 keV. Although an isothermal model can fit the thermal X-ray spectrum observed by RHESSI, such a model cannot account for the changes in altitude, and multi-thermal coronal sources are required where the temperature increases with altitude. For the first time, we show how RHESSI imaging information can be used to constrain the DEM(T) of a flaring plasma. We developed a thermal bremsstrahlung X-ray emission model with inhomogeneous temperature and density distributions to simultaneously reproduce i) DEM(T); ii) altitude as a function of energy; and iii) vertical extent of the flaring coronal source versus energy. We find that the temperature-altitude gradient in the region is similar to+0.08 keV/arcsec (similar to 1.3 MK/Mm). Similar altitude-energy trends in other flares suggest that the majority of coronal X-ray sources are multi-thermal and have strong vertical temperature and density gradients with a broad DEM(T).
C1 [Jeffrey, Natasha L. S.; Kontar, Eduard P.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Jeffrey, NLS (reprint author), Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
EM natasha.jeffrey@glasgow.ac.uk
RI Kontar, Eduard/B-7897-2008
OI Kontar, Eduard/0000-0002-8078-0902
FU STFC STEP award; STFC Consolidated Grant
FX N.L.S.J. was funded by a STFC STEP award. E.P.K. gratefully acknowledges
the financial support by the STFC Consolidated Grant.
NR 38
TC 0
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U1 0
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 DEC
PY 2015
VL 584
AR A89
DI 10.1051/0004-6361/201526665
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800089
ER
PT J
AU Lindberg, JE
Jorgensen, JK
Watanabe, Y
Bisschop, SE
Sakai, N
Yamamoto, S
AF Lindberg, J. E.
Jorgensen, J. K.
Watanabe, Y.
Bisschop, S. E.
Sakai, N.
Yamamoto, S.
TI Probing the effects of external irradiation on low-mass protostars
through unbiased line surveys
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: individual objects: R CrA; ISM: molecules;
astrochemistry; radiative transfer
ID CARBON-CHAIN-CHEMISTRY; YOUNG STELLAR OBJECTS; SPECTRAL
ENERGY-DISTRIBUTIONS; GRAIN SURFACE-CHEMISTRY; CORONA AUSTRALIS; IRAS
16293-2422; STAR-FORMATION; ORGANIC-MOLECULES; HOT CORE; DEUTERATED
MOLECULES
AB Context. The envelopes of molecular gas around embedded low-mass protostars show different chemistries, which can be used to trace their formation history and physical conditions. The excitation conditions of some molecular species can also be used to trace these physical conditions, making it possible to constrain for instance sources of heating and excitation.
Aims. We study the range of influence of an intermediate-mass Herbig Be protostar. We also study the effect of feedback from the environment on the chemical and physical properties of embedded protostars.
Methods. We followed up on an earlier line survey of the Class 0/I source R CrA IRS7B in the 0.8 mm window with an unbiased line survey of the same source in the 1.3 mm window using the Atacama Pathfinder Experiment (APEX) telescope. We also studied the excitation of the key species H2CO, CH3OH, and c-C3H2 in a complete sample of the 18 embedded protostars in the Corona Australis star-forming region. Radiative transfer models were employed to establish abundances of the molecular species.
Results. We detect line emission from 20 molecular species (32 including isotopologues) in the two surveys. The most complex species detected are CH3OH, CH3CCH, CH3CHO, and CH3CN (the latter two are only tentatively detected). CH3CN and several other complex organic molecules are significantly under-abundant in comparison with what is found towards hot corino protostars. The H2CO rotational temperatures of the sources in the region decrease with the distance to the Herbig Be star R CrA, whereas the c-C3H2 temperatures remain constant across the star-forming region.
Conclusions. The high H2CO temperatures observed towards objects close to R CrA suggest that this star has a sphere of influence of several 10 000 AU in which it increases the temperature of the molecular gas to 30-50 K through irradiation. The chemistry in the IRS7B envelope differs significantly from many other embedded protostars, which could be an effect of the external irradiation from R CrA.
C1 [Lindberg, J. E.; Jorgensen, J. K.; Bisschop, S. E.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Lindberg, J. E.; Jorgensen, J. K.; Bisschop, S. E.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark.
[Lindberg, J. E.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Watanabe, Y.; Sakai, N.; Yamamoto, S.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
RP Lindberg, JE (reprint author), Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.
EM johan.lindberg@nasa.gov
RI Sakai, Nami/N-7438-2015;
OI Sakai, Nami/0000-0002-3297-4497; Lindberg, Johan/0000-0003-3811-4591;
Watanabe, Yoshimasa/0000-0002-9668-3592
FU Danish National Research Foundation; University of Copenhagen's
programme of excellence; Lundbeck Foundation Group Leader Fellowship;
Ministry of Education, Culture, Sports, Science, and Technologies of
Japan [25108005]
FX We thank Steven Charnley for helpful suggestions and discussions. We
also thank the anonymous referee for helpful comments and suggestions
that have improved the manuscript. Research at Centre for Star and
Planet Formation is funded by the Danish National Research Foundation
and the University of Copenhagen's programme of excellence. This
research was also supported by an appointment to the NASA Postdoctoral
Program at the NASA Goddard Space Flight Center to J.E.L., administered
by Oak Ridge Associated Universities through a contract with NASA, and
by a Lundbeck Foundation Group Leader Fellowship to J.K.J. Y.W., N.S,
and S.Y. acknowledge financial support from Grant-in-Aid from the
Ministry of Education, Culture, Sports, Science, and Technologies of
Japan (25108005).
NR 78
TC 3
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U1 1
U2 2
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 DEC
PY 2015
VL 584
AR A28
DI 10.1051/0004-6361/201526222
PG 84
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800028
ER
PT J
AU Rambaux, N
Chambat, F
Castillo-Rogez, JC
AF Rambaux, N.
Chambat, F.
Castillo-Rogez, J. C.
TI Third-order development of shape, gravity, and moment of inertia for
highly flattened celestial bodies. Application to Ceres
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: fundamental parameters; planets and satellites:
individual: Ceres; methods: numerical
ID ROTATING LIQUID PLANETS; ADAPTIVE OPTICS IMAGES; ICY SATELLITES;
GRAVITATIONAL MOMENTS; ELLIPSOID DIMENSIONS; EVOLUTION; ASTEROIDS;
MODELS; EQUILIBRIUM; INTERIOR
AB Context. We investigate the hydrostatic shape and gravitational potential coefficients of self-gravitating and rotating bodies large enough to have undergone internal differentiation and chemical stratification. Quantifying these properties under the assumption of hydrostatic equilibrium forms the basis for interpreting shape and gravity data in terms of interior structure and infer deviations from hydrostaticity that can bring information on the thermal and chemical history of the objects.
Aims. The main purpose is to show the importance of developing the reference hydrostatic shape for relatively fast rotating bodies up to third order to reach an accuracy of a few tens of meters. This paper especially focuses on Ceres, for which high-resolution shape data are being obtained by the Dawn spacecraft, with a projected accuracy better than 200 m/pixel.
Methods. To improve the accuracy on the determination of geodetic parameters, we numerically integrated Clairaut's equations of rotational equilibrium expanded up to third order in a small parameter m, the geodetic parameter.
Results. Previous studies of Ceres have been based on shape models developed to first order. However, we show that the first-order theory underestimates (a - c) (where a and c are the equatorial and polar radii) by 1.8 km, which leads to underestimating the extent of mass concentration and is insufficient to interpret the upcoming observations by Dawn space mission. Instead, by using the third-order theory, we obtain an accuracy of 25 meters that is better than the accuracy expected from Dawn. Then, we derive the following geodetical quantities: flattening and other shape parameters, gravitational potential coefficients, and moments of inertia, by using the Ceres models constrained by observations obtained with the Hubble Space Telescope and ground-based adaptive optics telescopes. The difference in equatorial and polar radii for a large parametric space of interior models is investigated, and the large (a - c) corresponds to a model with a low density contrast.
Conclusions. This type of modeling will also prove instrumental to infer non-hydrostatic contributions to Ceres' shape that are to be measured by Dawn.
C1 [Rambaux, N.] Univ Lille 1, Univ Paris 06, Sorbonne Univ, IMCCE,Observ Paris,PSL Res Univ,CNRS, F-75014 Paris, France.
[Chambat, F.] ENS Lyon, CNRS, UMR5276, LGLTPE, F-69007 Lyon, France.
[Castillo-Rogez, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rambaux, N (reprint author), Univ Lille 1, Univ Paris 06, Sorbonne Univ, IMCCE,Observ Paris,PSL Res Univ,CNRS, 77 Ave Denfert Rochereau, F-75014 Paris, France.
EM Nicolas.Rambaux@obspm.fr
FU CNU through CRCT by the MESR [Sect. 34]
FX The authors are thankful to the anonymous referee for helpful comments.
N. Rambaux is grateful to the CNU, Sect. 34, for supporting a six-month
full-time research project through CRCT-2015 funding delivered by the
MESR. Part of this work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract to NASA.
NR 41
TC 2
Z9 2
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 DEC
PY 2015
VL 584
AR A127
DI 10.1051/0004-6361/201527005
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800126
ER
PT J
AU Sandqvist, A
Larsson, B
Hjalmarson, A
Encrenaz, P
Gerin, M
Goldsmith, PF
Lis, DC
Liseau, R
Pagani, L
Roueff, E
Viti, S
AF Sandqvist, Aa.
Larsson, B.
Hjalmarson, A.
Encrenaz, P.
Gerin, M.
Goldsmith, P. F.
Lis, D. C.
Liseau, R.
Pagani, L.
Roueff, E.
Viti, S.
TI Herschel HIFI observations of the Sgr A+50 km s(-1) Cloud Deep searches
for O-2 in emission and foreground absorption
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Galaxy: center; ISM: individual objects: Sgr A; ISM: molecules; ISM:
clouds
ID GIANT MOLECULAR CLOUDS; GALACTIC-CENTER; ODIN OBSERVATIONS; GASEOUS
STRUCTURE; DENSITY WAVES; SAGITTARIUS-A; RHO-OPHIUCHI; GALAXY M-83;
SPIRAL ARMS; GAS
AB Context. The Herschel Oxygen Project (HOP) is an open time key program, awarded 140 h of observing time to search for molecular oxygen (O-2) in a number of interstellar sources. To date O-2 has definitely been detected in only two sources, namely rho Oph A and Orion, reflecting the extremely low abundance of O-2 in the interstellar medium.
Aims. One of the sources in the HOP program is the + 50 km s(-1) Cloud in the Sgr A Complex in the centre of the Milky Way. Its environment is unique in the Galaxy and this property is investigated to see if it is conducive to the presence of O-2.
Methods. The Herschel Heterodyne Instrument for the Far Infrared (HIFI) is used to search for the 487 and 774 GHz emission lines of O-2.
Results. No O-2 emission is detected towards the Sgr A + 50 km s(-1) Cloud, but a number of strong emission lines of methanol (CH3OH) and absorption lines of chloronium (H2Cl+) are observed. Conclusions. A 3 sigma upper limit for the fractional abundance ratio of [O-2]/[H-2] in the Sgr A + 50 km s(-1) Cloud is found to be X(O-2) <= 5x 10(-8). However, since we can find no other realistic molecular candidate than O-2 itself, we very tentatively suggest that two weak absorption lines at 487.261 and 487.302 GHz may be caused by the 487 GHz line of O-2 in two foreground spiral arm clouds. By considering that the absorption may only be apparent, the estimated upper limit to the O-2 abundance of <=(10-20) x 10(-6) in these foreground clouds is very high, as opposed to the upper limit in the Sgr A + 50 km s(-1) Cloud itself, but similar to what has been reached in recent chemical shock models for Orion. This abundance limit was determined also using Odin non-detection limits, and assumes that O-2 fills the beam. If the absorption is due to a differential Herschel OFF-ON emission, the O-2 fractional abundance may be of the order of approximate to(5-10) x 10 (6). With the assumption of pure absorption by foreground clouds, the unreasonably high abundance of (1.4-2.8) x 10(-4) was obtained. The rotation temperatures for CH3OH-A and CH3OH-E lines in the + 50 km s(-1) Cloud are found to be approximate to 64 and 79 K, respectively, and the fractional abundance of CH3OH is approximately 5 x 10(-7).
C1 [Sandqvist, Aa.; Larsson, B.] Stockholm Univ, AlbaNova Univ Ctr, Stockholm Observ, S-10691 Stockholm, Sweden.
[Hjalmarson, A.; Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-42992 Onsala, Sweden.
[Encrenaz, P.; Lis, D. C.; Pagani, L.] Univ Paris 06, Univ Sorbonne, PSL Res Univ, Observ Paris,CNRS,LERMA, F-75014 Paris, France.
[Gerin, M.] Univ Paris 06, Ecole Normale Super, PSL Res Univ, Univ Sorbonne,CNRS,Observ Paris,LERMA, F-75005 Paris, France.
[Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Roueff, E.] Univ Paris 06, Univ Sorbonne, PSL Res Univ, Observ Paris,LERMA,CNRS, F-92190 Meudon, France.
[Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Sandqvist, A (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Stockholm Observ, S-10691 Stockholm, Sweden.
EM aage@astro.su.se
RI Goldsmith, Paul/H-3159-2016
FU Swedish National Space Board (SNSB); NASA through JPL/Caltech
FX We wish to thank Per Olof Lindblad for useful discussions and comments
concerning Galactic density waves and resulting shock interaction with
Galactic spiral arms. We are very grateful to our anonymous referee
whose thorough report significantly improved this paper. We also wish to
thank the Swedish National Space Board (SNSB) for its continued
financial support. Furthermore we express our appreciation to the
individuals making, updating and maintaining the Splatalogue, CDMS and
JPL molecular spectroscopy data bases for their unselfish demanding
work. HIFI has been designed and built by a consortium of institutes and
university departments from across Europe, Canada and the US under the
leadership of SRON Netherlands Institute for Space Research, Groningen,
The Netherlands 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; It aly:
ASI, IFSI-INAF, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK;
Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia
(CSIC-INTA); Sweden: Chalmers University of Technology MC2, RSS and
GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm
University Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA:
Caltech, JPL, NHSC. Support for this work was provided by NASA through
an award issued by JPL/Caltech.
NR 50
TC 1
Z9 1
U1 0
U2 0
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 DEC
PY 2015
VL 584
AR A118
DI 10.1051/0004-6361/201526280
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ2LN
UT WOS:000366936800118
ER
PT J
AU Poroseva, SV
Kaiser, BE
Sillero, JA
Murman, SM
AF Poroseva, S. V.
Kaiser, B. E.
Sillero, J. A.
Murman, S. M.
TI Validation of a closing procedure for fourth-order RANS turbulence
models with DNS data in an incompressible zero-pressure-gradient
turbulent boundary layer
SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW
LA English
DT Article
DE DNS; Boundary layer; High-order statistics; Gram-Charlier series
expansions
ID DIRECT NUMERICAL-SIMULATION; SPATIAL-RESOLUTION; REYNOLDS-NUMBER;
HOT-WIRE; VISCOUS SUBLAYER; SHEAR-STRESS; VELOCITY; FLOW; DISTRIBUTIONS;
PREDICTION
AB Among factors affecting the accuracy of flow simulations with Reynolds-Averaged Navier-Stokes turbulence models is modeling turbulent diffusion processes. With the use of the Gram-Charlier series expansions, the turbulent diffusion in fourth-order one-point statistical closures of the Reynolds-Averaged Navier-Stokes equations can be modeled without introducing unknown model coefficients and without assuming turbulence being Gaussian. Terms representing turbulent diffusion processes in transport equations for second- and third-order velocity correlations do not require any modeling in such closures. In this regard, fourth-order closures are a more accurate alternative to lower-order closures where turbulent diffusion is modeled on semi-empirical or Gaussian turbulence assumptions. In the current paper, the accuracy of the closing procedure based on the Gram-Charlier series expansions is evaluated using data of direct numerical simulations in an incompressible zero-pressure-gradient turbulent boundary layer over a flat plate. One-point third-, fourth-, and fifth-order velocity moments were extracted for this purpose from the dataset collected by the Fluid Dynamics Group at the Universidad Politecnica de Madrid at two streamwise locations Re-theta = 4101 and 5200 that correspond to channels and pipes at delta(+) 1331 and 1626. Results demonstrate that the truncated Gram-Charlier series expansions are an accurate approximation of the fifth-order velocity moments in the considered flow. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Poroseva, S. V.; Kaiser, B. E.] Univ New Mexico, Dept Mech Engn, Albuquerque, NM 87131 USA.
[Sillero, J. A.] Univ Politecn Madrid, Sch Aeronaut, E-28040 Madrid, Spain.
[Murman, S. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Poroseva, SV (reprint author), Univ New Mexico, Dept Mech Engn, Albuquerque, NM 87131 USA.
EM poroseva@unm.edu
FU National Aeronautics and Space Administration [NNX12AJ61A]; Junior
Faculty University of New Mexico - Los Alamos National Laboratory
Collaborative Research Grant
FX A part of the presented material is based upon work supported by
National Aeronautics and Space Administration under Award NNX12AJ61A and
by the Junior Faculty University of New Mexico - Los Alamos National
Laboratory Collaborative Research Grant. B.E. Kaiser and S.V. Poroseva
wish to thank the Center for Advance Research Computing at the
University of New Mexico for providing the access to high-performance
computing facilities and IT support.
NR 56
TC 0
Z9 0
U1 1
U2 2
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0142-727X
EI 1879-2278
J9 INT J HEAT FLUID FL
JI Int. J. Heat Fluid Flow
PD DEC
PY 2015
VL 56
BP 71
EP 79
DI 10.1016/j.ijheatfluidflow.2015.06.010
PG 9
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA CZ2VE
UT WOS:000366961900007
ER
PT J
AU Meneghini, R
Kim, H
Liao, L
Jones, JA
Kwiatkowski, JM
AF Meneghini, Robert
Kim, Hyokyung
Liao, Liang
Jones, Jeffrey A.
Kwiatkowski, John M.
TI An Initial Assessment of the Surface Reference Technique Applied to Data
from the Dual-Frequency Precipitation Radar (DPR) on the GPM Satellite
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID RAIN-PROFILING ALGORITHM; SPACEBORNE RADAR; RETRIEVAL ALGORITHM;
SINGLE-FREQUENCY; PATH ATTENUATION; CROSS-SECTIONS; AIRBORNE RADAR;
PERFORMANCE; OCEAN; BAND
AB It has long been recognized that path-integrated attenuation (PIA) can be used to improve precipitation estimates from high-frequency weather radar data. One approach that provides an estimate of this quantity from airborne or spaceborne radar data is the surface reference technique (SRT), which uses measurements of the surface cross section in the presence and absence of precipitation. Measurements from the dual-frequency precipitation radar (DPR) on the Global Precipitation Measurement (GPM) satellite afford the first opportunity to test the method for spaceborne radar data at Ka band as well as for the Ku-band-Ka-band combination.
The study begins by reviewing the basis of the single- and dual-frequency SRT. As the performance of the method is closely tied to the behavior of the normalized radar cross section (NRCS or sigma(0)) of the surface, the statistics of sigma(0) derived from DPR measurements are given as a function of incidence angle and frequency for ocean and land backgrounds over a 1-month period. Several independent estimates of the PIA, formed by means of different surface reference datasets, can be used to test the consistency of the method since, in the absence of error, the estimates should be identical. Along with theoretical considerations, the comparisons provide an initial assessment of the performance of the single- and dual-frequency SRT for the DPR. The study finds that the dual-frequency SRT can provide improvement in the accuracy of path attenuation estimates relative to the single-frequency method, particularly at Ku band.
C1 [Meneghini, Robert; Kwiatkowski, John M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kim, Hyokyung; Liao, Liang] Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA.
[Kim, Hyokyung; Liao, Liang] Morgan State Univ, Baltimore, MD 21239 USA.
[Jones, Jeffrey A.] Wyle, Sci Technol & Engn Grp, Greenbelt, MD USA.
[Kwiatkowski, John M.] George Mason Univ, Fairfax, VA 22030 USA.
RP Meneghini, R (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
RI Measurement, Global/C-4698-2015
FU NASA [NNH12ZDA001N-PMM]
FX We wish to thank members of the JAXA and NASA data processing teams for
providing the data. This work is supported by Dr. Ramesh Kakar of NASA
headquarters under NASA Grant NNH12ZDA001N-PMM.
NR 31
TC 3
Z9 3
U1 3
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD DEC
PY 2015
VL 32
IS 12
BP 2281
EP 2296
DI 10.1175/JTECH-D-15-0044.1
PG 16
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CZ3FH
UT WOS:000366989300002
ER
PT J
AU Smith, SM
Zwart, SR
AF Smith, Scott M.
Zwart, Sara R.
TI Magnesium and Space Flight
SO NUTRIENTS
LA English
DT Article
DE microgravity; bone; tissue magnesium; bed rest
ID LONG-DURATION SPACEFLIGHT; DOWN BED REST; BONE-MINERAL BALANCE; STABLE
CALCIUM ISOTOPES; NUTRITIONAL-STATUS; INSULIN-RESISTANCE; OXIDATIVE
DAMAGE; TISSUE MAGNESIUM; BLOOD-PRESSURE; STONE RISK
AB Magnesium is an essential nutrient for muscle, cardiovascular, and bone health on Earth, and during space flight. We sought to evaluate magnesium status in 43 astronauts (34 male, 9 female; 47 +/- 5 years old, mean +/- SD) before, during, and after 4-6-month space missions. We also studied individuals participating in a ground analog of space flight (head-down-tilt bed rest; n = 27 (17 male, 10 female), 35 +/- 7 years old). We evaluated serum concentration and 24-h urinary excretion of magnesium, along with estimates of tissue magnesium status from sublingual cells. Serum magnesium increased late in flight, while urinary magnesium excretion was higher over the course of 180-day space missions. Urinary magnesium increased during flight but decreased significantly at landing. Neither serum nor urinary magnesium changed during bed rest. For flight and bed rest, significant correlations existed between the area under the curve of serum and urinary magnesium and the change in total body bone mineral content. Tissue magnesium concentration was unchanged after flight and bed rest. Increased excretion of magnesium is likely partially from bone and partially from diet, but importantly, it does not come at the expense of muscle tissue stores. While further study is needed to better understand the implications of these findings for longer space exploration missions, magnesium homeostasis and tissue status seem well maintained during 4-6-month space missions.
C1 [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
[Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov; sara.zwart-1@nasa.gov
FU NASA Human Health Countermeasure Element of the Human Research Program;
Institute for Translational Sciences at the University of Texas Medical
Branch - Clinical and Translational Science Award from the National
Center for Advancing Translational Sciences, National Institutes of
Health [UL1TR000071]
FX We thank the astronauts for their participation in and support of this
study. We thank the staff of the NASA Johnson Space Center Nutritional
Biochemistry Laboratory for their assistance in all aspects of carrying
out this project. We thank the International Space Station Medical
Project, the Flight Analogs Project, and the NASA Lifetime Surveillance
of Astronaut Health team for their help with these studies and data
reported herein. We thank Peter Norsk for helpful discussions regarding
these findings. We thank Jane Krauhs for editorial assistance. This
study was funded by the NASA Human Health Countermeasure Element of the
Human Research Program. This study was conducted with the support of the
Institute for Translational Sciences at the University of Texas Medical
Branch, supported in part by a Clinical and Translational Science Award
(UL1TR000071) from the National Center for Advancing Translational
Sciences, National Institutes of Health.
NR 66
TC 1
Z9 1
U1 1
U2 10
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-6643
J9 NUTRIENTS
JI Nutrients
PD DEC
PY 2015
VL 7
IS 12
BP 10209
EP 10222
DI 10.3390/nu7125528
PG 14
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA CZ4DA
UT WOS:000367052200035
PM 26670248
ER
PT J
AU Sugawara, Y
Maeda, Y
Tsuboi, Y
Hamaguchi, K
Corcoran, M
Pollock, AMT
Moffat, AFJ
Williams, PM
Dougherty, S
Pittard, J
AF Sugawara, Yasuharu
Maeda, Yoshitomo
Tsuboi, Yohko
Hamaguchi, Kenji
Corcoran, Michael
Pollock, Andy M. T.
Moffat, Anthony F. J.
Williams, Peredur M.
Dougherty, Sean
Pittard, Julian
TI Suzaku monitoring of the Wolf-Rayet binary WR140 around periastron
passage: An approach for quantifying the wind parameters
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE binaries: eclipsing; stars: winds, outflows; stars: Wolf-Rayet; X-rays:
individual (WR 140)
ID EARLY-TYPE STARS; X-RAY; WR 140; BOARD SUZAKU; MULTIFREQUENCY
VARIATIONS; RADIO OBSERVATIONS; LINE DIAGNOSTICS; IN-ORBIT; EMISSION;
SYSTEM
AB Suzaku observations of theWolf-Rayet (W-R) binaryWR 140 (WC7pd+O5.5fc) were made at four different times around periastron passage in 2009 January. The spectra changed in shape and flux with the phase. As periastron approached, the column density of the low-energy absorption increased, which indicates that the emission from the wind-wind collision plasma was absorbed by the dense W-R wind. The spectra can be mostly fitted with two different components: a warm component with k(B)T = 0.3-0.6 keV and a dominant hot component with k(B)T similar to 3 keV. The emission measure of the dominant, hot component is not inversely proportional to the distance between the two stars. This can be explained by the O star wind colliding before it has reached its terminal velocity, leading to a reduction in its wind momentum flux. At phases closer to periastron, we discovered a cool plasma component in a recombining phase, which is less absorbed. This component may be a relic of the wind-wind collision plasma, which was cooled down by radiation, and may represent a transitional stage in dust formation.
C1 [Sugawara, Yasuharu; Tsuboi, Yohko] Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan.
[Maeda, Yoshitomo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2298510, Japan.
[Maeda, Yoshitomo] SOKENDAI, Dept Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Hamaguchi, Kenji; Corcoran, Michael] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji; Corcoran, Michael] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Corcoran, Michael] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Pollock, Andy M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, Madrid 28691, Spain.
[Pollock, Andy M. T.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Moffat, Anthony F. J.] Ctr Rech Astrophys Quebec, Quebec City, PQ, Canada.
[Williams, Peredur M.] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dougherty, Sean] Natl Res Council Canada, DRAO, Penticton, BC V2A 6J9, Canada.
[Pittard, Julian] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
RP Sugawara, Y (reprint author), Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, 1-13-27 Kasuga, Tokyo 1128551, Japan.
EM sugawara@phys.chuo-u.ac.jp
OI Pittard, Julian/0000-0003-2244-5070
FU Japan Society for the Promotion of Science; Ministry of Education,
Culture, Sports, Science and Technology [20540237, 21018009, 23540269,
23540280]; Chuo University Grant for Special Research; NASA's
Astrobiology Institute [RTOP 344-53-51]; NSERC (Canada); FQRNT (Quebec);
Royal Society
FX We thank the referee for their help in improving the quality of this
paper. We also thank M. Sakano for his invaluable help. This research
has made use of data and/or software provided by 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. Y.S. acknowledges financial support from the Japan Society
for the Promotion of Science. Y.T. and Y.M. acknowledge support from the
Grants-in-Aid for Scientific Research (numbers 20540237, 21018009,
23540269, and 23540280) by the Ministry of Education, Culture, Sports,
Science and Technology. Y.T. also acknowledges financial support by a
Chuo University Grant for Special Research. K.H. is grateful for
financial support by the NASA's Astrobiology Institute (RTOP 344-53-51)
to the Goddard Center for Astrobiology. A.F.J.M. is grateful for
financial aid from NSERC (Canada) and FQRNT (Quebec). P.M.W. is grateful
to the Institute for Astronomy for continued hospitality and access to
the facilities of the Royal Observatory. J.M.P. would like to thank the
Royal Society for funding a University Research Fellowship. This
research has made use of NASA's Astrophysics Data System.
NR 49
TC 2
Z9 2
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 DEC
PY 2015
VL 67
IS 6
AR 121
DI 10.1093/pasj/psv099
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CZ1IQ
UT WOS:000366859800021
ER
PT J
AU Mirletz, BT
Bhandal, P
Adams, RD
Agogino, AK
Quinn, RD
SunSpiral, V
AF Mirletz, Brian T.
Bhandal, Perry
Adams, Ryan D.
Agogino, Adrian K.
Quinn, Roger D.
SunSpiral, Vytas
TI Goal-Directed CPG-Based Control for Tensegrity Spines with Many Degrees
of Freedom Traversing Irregular Terrain
SO SOFT ROBOTICS
LA English
DT Article
ID LOCOMOTION; MODEL; ROBOT; SIMULATION; OSCILLATORS; ENTRAINMENT;
ADAPTATION; GENERATION; HYPOTHESIS; LAMPREY
AB To further the ability of robots to achieve goals in environments with irregular terrain, we have developed a series of tensegrity spines as an abstraction of the many degrees of freedom (DOF) compliant spines seen in nature, with full six DOF between vertebrae (constrained by a tensile network). This work provides insight into control strategies for such many DOF and compliant systems, which lack the rigidly connected segments needed by traditional control. Our Central Pattern Generator (CPG)-based controller receives both proprioceptive feedback and goal-directed input. We utilize artificial neural networks to process both the feedback and the input, and only use feedback available to our analogous robotic hardware. This approach seeks to maximize the low-level competence of the control system, by combining local reflexes with structural compliance. This is, to our knowledge, the first example of a robot controlled by CPGs that is simultaneously capable of goal-directed behavior and locomotion on irregular terrain. In addition, this is the first goal-directed controller for a tensegrity robot that can transition between different terrains.
C1 [Mirletz, Brian T.; Quinn, Roger D.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
[Bhandal, Perry] Queens Univ, Sch Comp, Kingston, ON, Canada.
[Adams, Ryan D.] Cyan Data Syst, Oakland, CA USA.
[Agogino, Adrian K.] NASA, Ames Res Ctr, Robust Software Engn Grp, Moffett Field, CA 94035 USA.
[SunSpiral, Vytas] NASA, Ames Res Ctr, Intelligent Robot Grp, Moffett Field, CA 94035 USA.
RP SunSpiral, V (reprint author), NASA, Ames Res Ctr, MS N269-3, Moffett Field, CA 94035 USA.
EM vytas.sunspiral@nasa.gov
FU NASA Space Technology Research Fellowship [NNX11AN15H]; NASA Innovative
Advanced Concepts Program
FX The authors thank Tom Flemons and Stephen Levin for inspiration on
biotensegrity, John Chris Adams for computational support, and Dorothea
Blostein for comments on drafts. This work was supported by a NASA Space
Technology Research Fellowship (No. NNX11AN15H) and the NASA Innovative
Advanced Concepts Program.
NR 57
TC 1
Z9 1
U1 4
U2 13
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 2169-5172
EI 2169-5180
J9 SOFT ROBOT
JI Soft Robot.
PD DEC
PY 2015
VL 2
IS 4
BP 165
EP 176
DI 10.1089/soro.2015.0012
PG 12
WC Robotics
SC Robotics
GA CZ6UK
UT WOS:000367236300006
ER
PT J
AU Ryan, SJ
McNally, A
Johnson, LR
Mordecai, EA
Ben-Horin, T
Paaijmans, K
Lafferty, KD
AF Ryan, Sadie J.
McNally, Amy
Johnson, Leah R.
Mordecai, Erin A.
Ben-Horin, Tal
Paaijmans, Krijn
Lafferty, Kevin D.
TI Mapping Physiological Suitability Limits for Malaria in Africa Under
Climate Change
SO VECTOR-BORNE AND ZOONOTIC DISEASES
LA English
DT Article
DE Malaria; Climate change; Physiological response; Africa
ID VECTOR-BORNE DISEASES; PLASMODIUM-FALCIPARUM; INFECTIOUS-DISEASES;
TRANSMISSION INTENSITY; TEMPERATURE-VARIATION; SOUTH-AFRICA; HIGHLANDS;
VIVAX; RATES; RISK
AB We mapped current and future temperature suitability for malaria transmission in Africa using a published model that incorporates nonlinear physiological responses to temperature of the mosquito vector Anopheles gambiae and the malaria parasite Plasmodium falciparum. We found that a larger area of Africa currently experiences the ideal temperature for transmission than previously supposed. Under future climate projections, we predicted a modest increase in the overall area suitable for malaria transmission, but a net decrease in the most suitable area. Combined with human population density projections, our maps suggest that areas with temperatures suitable for year-round, highest-risk transmission will shift from coastal West Africa to the Albertine Rift between the Democratic Republic of Congo and Uganda, whereas areas with seasonal transmission suitability will shift toward sub-Saharan coastal areas. Mapping temperature suitability places important bounds on malaria transmissibility and, along with local level demographic, socioeconomic, and ecological factors, can indicate where resources may be best spent on malaria control.
C1 [Ryan, Sadie J.] Univ Florida, Dept Geog, Gainesville, FL 32611 USA.
[Ryan, Sadie J.] Univ Florida, Emerging Pathogens Inst, Gainesville, FL 32611 USA.
[Ryan, Sadie J.] SUNY Upstate Med Univ, Dept Immunol & Microbiol, Ctr Global Hlth & Translat Sci, Syracuse, NY 13210 USA.
[Ryan, Sadie J.] Univ KwaZulu Natal, Coll Agr Engn & Sci, Sch Life Sci, Durban, South Africa.
[McNally, Amy] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Johnson, Leah R.] Univ S Florida, Div Integrat Biol, Tampa, FL USA.
[Mordecai, Erin A.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA.
[Ben-Horin, Tal] Rutgers State Univ, Dept Marine & Coastal Sci, New Brunswick, NJ 08903 USA.
[Paaijmans, Krijn] Hosp Clin Univ Barcelona, Barcelona Ctr Int Hlth Res CRESIB, ISGlobal, Barcelona, Spain.
[Lafferty, Kevin D.] Univ Calif Santa Barbara, Inst Marine Sci, Western Ecol Res Ctr, US Geol Survey, Santa Barbara, CA 93106 USA.
[Lafferty, Kevin D.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
RP Ryan, SJ (reprint author), Univ Florida, Dept Geog, 3128 Turlington Hall, Gainesville, FL 32611 USA.
EM sjryan@ufl.edu
OI Ryan, Sadie/0000-0002-4308-6321
FU Luce Environmental Science to Solutions Fellowship; National Center for
Ecological Analysis and Synthesis; National Science Foundation
[EF-0553768]; University of California, Santa Barbara; State of
California; National Science Foundation Postdoctoral Research Fellowship
in Biology [DBI-1202892]
FX This work was conducted as a part of the Malaria and Climate Change
Working Group supported by the Luce Environmental Science to Solutions
Fellowship and the National Center for Ecological Analysis and
Synthesis, a Center funded by the National Science Foundation (grant no.
EF-0553768), the University of California, Santa Barbara, and the State
of California. Greg Husak and Bobby Gramacy provided input on data
acquisition. E.A.M. was supported by a National Science Foundation
Postdoctoral Research Fellowship in Biology (DBI-1202892). Any use of
trade, product, website, or firm names in this publication is for
descriptive purposes only and does not imply endorsement by the US
Government.
NR 44
TC 3
Z9 3
U1 9
U2 41
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1530-3667
EI 1557-7759
J9 VECTOR-BORNE ZOONOT
JI Vector-Borne Zoonotic Dis.
PD DEC 1
PY 2015
VL 15
IS 12
BP 718
EP 725
DI 10.1089/vbz.2015.1822
PG 8
WC Public, Environmental & Occupational Health; Infectious Diseases
SC Public, Environmental & Occupational Health; Infectious Diseases
GA CY9JS
UT WOS:000366723800002
PM 26579951
ER
PT J
AU Schultz, CJ
Carey, LD
Schultz, EV
Blakeslee, RJ
AF Schultz, Christopher J.
Carey, Lawrence D.
Schultz, Elise V.
Blakeslee, Richard J.
TI Insight into the Kinematic and Microphysical Processes that Control
Lightning Jumps
SO WEATHER AND FORECASTING
LA English
DT Article
ID MESOSCALE CONVECTIVE SYSTEM; DOPPLER RADAR OBSERVATIONS; REAL-TIME;
SIMULATED ELECTRIFICATION; PRECIPITATION DEVELOPMENT; MULTIPARAMETER
RADAR; SEVERE THUNDERSTORMS; DETECTION ALGORITHM; POLARIMETRIC RADAR;
SUPERCELL STORM
AB A detailed case study analysis of four thunderstorms is performed using polarimetric and multi-Doppler capabilities to provide specificity on the physical and dynamical drivers behind lightning jumps. The main differences between small increases in the total flash rate and a lightning jump are the increases in graupel mass and updraft volumes 10 m s(-1) between the -10 degrees and -40 degrees C isotherms. Updraft volumes >= 10 m s(-1) increased in magnitude at least 3-5 min in advance of the increase in both graupel mass and total flash rate. Updraft volumes >= 10 m s(-1) are more robustly correlated to total flash rate than maximum updraft speed over a thunderstorm's entire life cycle. However, peak updraft speeds increase prior to 8 of the 12 lightning jumps examined. Decreases in mean and median flash footprint size during increases in total lightning are observed in all four thunderstorms and are most notable during development stages within the most intense storms. However, this inverse relationship breaks down on larger storm scales as storms mature and anvils and stratiform regions developed with time. Promisingly, smaller flash sizes are still collocated with the strongest updraft speeds, while larger flash sizes are observed within weaker updraft regions. The results herein emphasize the following for lightning jump applications: both the lightning jump sigma level and the resultant magnitude of the total flash rate must be employed in conjunction to assess storm intensity using lightning data. The sigma-level magnitude of the lightning jump is the early warning that indicates that rapid intensification is occurring, while the magnitude of the total flash rate provides insight into the size and maintenance of the updraft volume and graupel mass. These cases serve as conceptual models for future applications of the lightning jump algorithm for hazardous weather monitoring.
C1 [Schultz, Christopher J.; Carey, Lawrence D.] Univ Alabama, Dept Atmospher Sci, Tuscaloosa, AL 35487 USA.
[Schultz, Christopher J.; Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Schultz, Elise V.] Univ Alabama, Ctr Earth Syst Sci, Tuscaloosa, AL 35487 USA.
RP Schultz, CJ (reprint author), UAH NASA MSFC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM christopher.j.schultz@nasa.gov
FU NOAA/NASA GOES-R Risk Reduction Research
FX The authors would like to acknowledge Dr. Steven J. Goodman and
NOAA/NASA GOES-R Risk Reduction Research funding for support of this
research. CJS would like to acknowledge support from the NASA Pathways
Intern Program at Marshall Space Flight Center, namely Julie Clift and
Christopher Randall. The authors are thankful for technical support with
radar data processing from Lamont Bain, Retha Mecikalski, and Danielle
Kozlowski for parts of the 11 June and 10 April events. The authors
would like to also acknowledge Dr. Walt Petersen for directing the
collection of ARMOR data during his tenure at the Earth System Science
Center and NASA MSFC in Huntsville. Furthermore, productive
conversations with Themis Chronis, Phil Bitzer, Hugh Christian, and
Kristin Calhoun benefited the outcomes of this research. We also
gratefully acknowledge the technical support for maintenance of the
operational instrumentation, namely Dustin Phillips, Patrick Gatlin, and
Chris Phillips for the maintenance of ARMOR, and Jeff Bailey for the
continued maintenance of the North Alabama Lightning Mapping Array.
Finally, we thank Dr. Eric Bruning and two anonymous reviewers for
thorough and constructive reviews that improved this article.
NR 75
TC 9
Z9 9
U1 1
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
EI 1520-0434
J9 WEATHER FORECAST
JI Weather Forecast.
PD DEC
PY 2015
VL 30
IS 6
BP 1591
EP 1621
DI 10.1175/WAF-D-14-00147.1
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CZ3EB
UT WOS:000366986100001
ER
PT J
AU Gully-Santiago, M
Jaffe, DT
White, V
AF Gully-Santiago, Michael
Jaffe, Daniel T.
White, Victor
TI Optical characterization of gaps in directly bonded Si compound optics
using infrared spectroscopy
SO APPLIED OPTICS
LA English
DT Article
ID INTERNAL-REFLECTION SPECTROSCOPY; ROOM-TEMPERATURE; SILICON-WAFERS;
ABSORPTION; ENVIRONMENT; DYNAMICS
AB Silicon direct bonding offers flexibility in the design and development of Si optics by allowing manufacturers to combine subcomponents with a potentially lossless and mechanically stable interface. The bonding process presents challenges in meeting the requirements for optical performance because air gaps at the Si interface cause large Fresnel reflections. Even small (35 nm) gaps reduce transmission through a direct bonded Si compound optic by 4% at lambda = 1.25 mu m at normal incidence. We describe a bond inspection method that makes use of precision slit spectroscopy to detect and measure gaps as small as 14 nm. Our method compares low-finesse Fabry-Perot models to high-precision measurements of transmission as a function of wavelength. We demonstrate the validity of the approach by measuring bond gaps of known depths produced by microlithography. (C) 2015 Optical Society of America
C1 [Gully-Santiago, Michael; Jaffe, Daniel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[White, Victor] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gully-Santiago, M (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM gully@astro.as.utexas.edu
OI Gully-Santiago, Michael/0000-0002-4020-3457
FU National Aeronautics and Space Administration (NASA) [NNX10AK82H,
NNX12AC31G]
FX National Aeronautics and Space Administration (NASA) (NNX10AK82H,
NNX12AC31G).
NR 36
TC 2
Z9 2
U1 1
U2 1
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 DEC 1
PY 2015
VL 54
IS 34
BP 10177
EP 10188
DI 10.1364/AO.54.010177
PG 12
WC Optics
SC Optics
GA CY7QW
UT WOS:000366604800023
PM 26836675
ER
PT J
AU Scharf, C
Virgo, N
Cleaves, HJ
Aono, M
Aubert-Kato, N
Aydinoglu, A
Barahona, A
Barge, LM
Benner, SA
Biehl, M
Brasser, R
Butch, CJ
Chandru, K
Cronin, L
Danielache, S
Fischer, J
Hernlund, J
Hut, P
Ikegami, T
Kimura, J
Kobayashi, K
Mariscal, C
McGlynn, S
Menard, B
Packard, N
Pascal, R
Pereto, J
Rajamani, S
Sinapayen, L
Smith, E
Switzer, C
Takai, K
Tian, F
Ueno, Y
Voytek, M
Witkowski, O
Yabuta, H
AF Scharf, Caleb
Virgo, Nathaniel
Cleaves, H. James
Aono, Masashi
Aubert-Kato, Nathanael
Aydinoglu, Arsev
Barahona, Ana
Barge, Laura M.
Benner, Steven A.
Biehl, Martin
Brasser, Ramon
Butch, Christopher J.
Chandru, Kuhan
Cronin, Leroy
Danielache, Sebastian
Fischer, Jakob
Hernlund, John
Hut, Piet
Ikegami, Takashi
Kimura, Jun
Kobayashi, Kensei
Mariscal, Carlos
McGlynn, Shawn
Menard, Brice
Packard, Norman
Pascal, Robert
Pereto, Juli
Rajamani, Sudha
Sinapayen, Lana
Smith, Eric
Switzer, Christopher
Takai, Ken
Tian, Feng
Ueno, Yuichiro
Voytek, Mary
Witkowski, Olaf
Yabuta, Hikaru
TI A Strategy for Origins of Life Research
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 [Scharf, Caleb] Columbia Univ, New York, NY USA.
[Virgo, Nathaniel; Cleaves, H. James; Aono, Masashi; Brasser, Ramon; Chandru, Kuhan; Hernlund, John; Hut, Piet; Kimura, Jun; Packard, Norman; Smith, Eric; Ueno, Yuichiro] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528550, Japan.
[Cleaves, H. James; Hut, Piet] Inst Adv Study, Princeton, NJ 08540 USA.
[Aubert-Kato, Nathanael] Ochanomizu Univ, Tokyo 112, Japan.
[Aydinoglu, Arsev] Middle E Tech Univ, TR-06531 Ankara, Turkey.
[Barahona, Ana] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico.
[Barge, Laura M.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Benner, Steven A.] Fdn Appl Mol Evolut, Gainesville, FL USA.
[Biehl, Martin; Sinapayen, Lana] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
[Biehl, Martin; Fischer, Jakob; Ikegami, Takashi; Witkowski, Olaf] Univ Tokyo, Tokyo, Japan.
[Butch, Christopher J.] Tokyo Inst Technol, ELSI Origins Network EON, Earth Life Sci Inst, Tokyo 1528550, Japan.
[Butch, Christopher J.] Emory Univ, Atlanta, GA 30322 USA.
[Cronin, Leroy] Univ Glasgow, Glasgow, Lanark, Scotland.
[Danielache, Sebastian] Sophia Univ, Tokyo 102, Japan.
[Kobayashi, Kensei] Yokohama Natl Univ, Yokohama, Kanagawa 240, Japan.
[Mariscal, Carlos] Dalhousie Univ, Halifax, NS, Canada.
[McGlynn, Shawn] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Menard, Brice] Johns Hopkins Univ, Baltimore, MD USA.
[Packard, Norman] ProtoLife, Venice, Italy.
[Pascal, Robert] Univ Montpellier, CNRS, F-34059 Montpellier, France.
[Pereto, Juli] Univ Valencia, Valencia, Spain.
[Rajamani, Sudha] Indian Inst Sci Educ & Res, Pune, Maharashtra, India.
[Switzer, Christopher] Univ Calif Riverside, Riverside, CA 92521 USA.
[Takai, Ken] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Yokosuka, Kanagawa, Japan.
[Tian, Feng] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
[Voytek, Mary] NASA, Astrobiol Program, Washington, DC 20546 USA.
[Yabuta, Hikaru] Osaka Univ, Osaka, Germany.
[Fischer, Jakob] Univ Jena, Jena, Germany.
RP Cleaves, HJ (reprint author), Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, 2-12-1-IE-1 Ookayama, Tokyo 1528550, Japan.
EM henderson.cleaves@gmail.com
RI Pereto, Juli/G-5969-2015; Pascal, Robert/O-1559-2013; Kimura,
Jun/D-6050-2013; Aono, Masashi/A-7275-2014; Yabuta, Hikaru/M-9041-2014;
Hernlund, John/A-8931-2014;
OI Cronin, Lee/0000-0001-8035-5757; Cleaves, Henderson/0000-0003-4101-0654;
Pereto, Juli/0000-0002-5756-1517; Pascal, Robert/0000-0001-9579-2503;
Kimura, Jun/0000-0002-5825-0454; Aono, Masashi/0000-0001-8676-9643;
Yabuta, Hikaru/0000-0002-4625-5362; Hernlund, John/0000-0003-1008-0182;
Virgo, Nathaniel/0000-0001-8598-590X; Witkowski,
Olaf/0000-0002-2101-2428; Butch, Christopher/0000-0003-3112-0470
NR 22
TC 3
Z9 3
U1 9
U2 49
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 DEC 1
PY 2015
VL 15
IS 12
BP 1031
EP 1042
DI 10.1089/ast.2015.1113
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CY9JF
UT WOS:000366722500001
PM 26684503
ER
PT J
AU Onofri, S
de Vera, JP
Zucconi, L
Selbmann, L
Scalzi, G
Venkateswaran, KJ
Rabbow, E
de la Torre, R
Horneck, G
AF Onofri, Silvano
de Vera, Jean-Pierre
Zucconi, Laura
Selbmann, Laura
Scalzi, Giuliano
Venkateswaran, Kasthuri J.
Rabbow, Elke
de la Torre, Rosa
Horneck, Gerda
TI Survival of Antarctic Cryptoendolithic Fungi in Simulated Martian
Conditions On Board the International Space Station
SO ASTROBIOLOGY
LA English
DT Article
DE Endoliths; Eukaryotes; Extremophilic microorganisms; Mars; Radiation
resistance
ID LOW-EARTH-ORBIT; EXPOSE-R FACILITY; DESERT CYANOBACTERIUM
CHROOCOCCIDIOPSIS; COSMIC-RADIATION EXPOSURE; AMINO EXPERIMENT; E
MISSION; BLACK FUNGI; OUTER-SPACE; MARS; LIFE
AB Dehydrated Antarctic cryptoendolithic communities and colonies of the rock inhabitant black fungi Cryomyces antarcticus (CCFEE 515) and Cryomyces minteri (CCFEE 5187) were exposed as part of the Lichens and Fungi Experiment (LIFE) for 18 months in the European Space Agency's EXPOSE-E facility to simulated martian conditions aboard the International Space Station (ISS). Upon sample retrieval, survival was proved by testing colony-forming ability, and viability of cells (as integrity of cell membrane) was determined by the propidium monoazide (PMA) assay coupled with quantitative PCR tests. Although less than 10% of the samples exposed to simulated martian conditions were able to proliferate and form colonies, the PMA assay indicated that more than 60% of the cells and rock communities had remained intact after the Mars exposure. Furthermore, a high stability of the DNA in the cells was demonstrated. The results contribute to assessing the stability of resistant microorganisms and biosignatures on the surface of Mars, data that are valuable information for further search-for-life experiments on Mars.
C1 [Onofri, Silvano; Zucconi, Laura; Selbmann, Laura; Scalzi, Giuliano] Univ Tuscia, Dept Ecol & Biol Sci, I-01100 Viterbo, Italy.
[de Vera, Jean-Pierre] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[Venkateswaran, Kasthuri J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rabbow, Elke; Horneck, Gerda] German Aerosp Ctr DLR, Inst Aerosp Med, Cologne, Germany.
[de la Torre, Rosa] Spanish Aerosp Res Estab INTA, Dept Earth Observat, Madrid, Spain.
RP Onofri, S (reprint author), Univ Tuscia, Dept Ecol & Biol Sci, I-01100 Viterbo, Italy.
EM onofri@unitus.it
OI Zucconi, Laura/0000-0001-9793-2303
FU Italian National Program of Antarctic Researches (PNRA); Italian
National Antarctic Museum; German Ministry of Economy and Technology
BMWi; HGF-Foundation
FX The European Space Agency is acknowledged for the provision and
operations of the EXPOSE-E facility. We also thank the Italian National
Program of Antarctic Researches (PNRA) and Italian National Antarctic
Museum for funding the collection of Antarctic samples, the preservation
of the Culture Collection of Fungi from Extreme Environments (CCFEE),
and sample analyses. Special thanks are also due to the German Ministry
of Economy and Technology BMWi as well as to the HGF-Foundation in the
frame of the Helmholtz-Alliance "Planetary Evolution and Life,'' which
have partly supported the German Co-Is of this work.
NR 45
TC 2
Z9 2
U1 6
U2 30
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 DEC 1
PY 2015
VL 15
IS 12
BP 1052
EP 1059
DI 10.1089/ast.2015.1324
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CY9JF
UT WOS:000366722500003
PM 26684504
ER
PT J
AU Burgasser, AJ
Melis, C
Todd, J
Gelino, CR
Hallinan, G
Gagliuffi, DB
AF Burgasser, Adam J.
Melis, Carl
Todd, Jacob
Gelino, Christopher R.
Hallinan, Gregg
Gagliuffi, Daniella Bardalez
TI RADIO EMISSION AND ORBITAL MOTION FROM THE CLOSE-ENCOUNTER STAR-BROWN
DWARF BINARY WISE J072003.20-084651.2
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: visual; brown dwarfs; stars: chromospheres; stars: individual
(WISE J072003.20-084651.2); stars: low-mass; stars: magnetic field
ID ADAPTIVE OPTICS SYSTEM; INFRARED FILTER SET; LOW-MASS BINARIES;
MAIN-SEQUENCE; T-DWARF; MAGNETIC ACTIVITY; ULTRACOOL DWARFS; DYNAMICAL
MASS; SKY SURVEY; ROTATION
AB We report the detection of radio emission and orbital motion from the nearby star-brown dwarf binary WISE J072003.20-084651.2AB. Radio observations across the 4.5-6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15 +/- 3 mu Jy, and a highly polarized radio source that underwent a 2-3 minute burst with peak flux density 300 +/- 90 mu Jy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band Ha monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional orbital motion. We used these data to revise our estimates for the orbital period (4.1(-1.3) (+2.7) year) and tightly constrain the orbital inclination to be nearly edge-on (93 degrees.6(-1.degrees 4)(+1.degrees 6)), although robust measures of the component and system masses will require further monitoring. The inferred orbital motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
C1 [Burgasser, Adam J.; Melis, Carl; Gagliuffi, Daniella Bardalez] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Todd, Jacob] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Gelino, Christopher R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Gelino, Christopher R.; Hallinan, Gregg] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Burgasser, AJ (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
EM aburgasser@ucsd.edu
FU National Science Foundation [AST-1313428]; National Aeronautics and
Space Administration [NNX15AI75G]; Google; W. M. Keck Foundation
FX The authors thank Randy Campbell, Heather Hershley, and Marc Kassis at
Keck Observatory; and Pavl Zachary and Shawn Stone at Lick Observatory
for their assistance with the observations. We thank our anonymous
referee for her/his/their helpful comments, particularly on the MCMC
analysis. C. M. acknowledges funding support from the National Science
Foundation under award No. AST-1313428. The material is based upon work
supported by the National Aeronautics and Space Administration under
Grant No. NNX15AI75G. This research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France; NASA's Astrophysics Data System
Bibliographic Services; the M, L, T, and Y dwarf compendium housed at
DwarfArchives.org; and the SpeX Prism Libraries at
http://www.browndwarfs.org/spexprism. Research at Lick Observatory is
partially supported by a generous gift from Google. The authors
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate and grateful to
have the opportunity to conduct observations from this mountain.; 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 Observatory was made
possible by the generous financial support of the W. M. Keck Foundation.
NR 57
TC 5
Z9 5
U1 0
U2 0
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 DEC
PY 2015
VL 150
IS 6
AR 180
DI 10.1088/0004-6256/150/6/180
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY7KZ
UT WOS:000366588600015
ER
PT J
AU Hartman, JD
Bhatti, W
Bakos, GA
Bieryla, A
Kovacs, G
Latham, DW
Csubry, Z
de Val-Borro, M
Penev, K
Buchhave, LA
Torres, G
Howard, AW
Marcy, GW
Johnson, JA
Isaacson, H
Sato, B
Boisse, I
Falco, E
Everett, ME
Szklenar, T
Fulton, BJ
Shporer, A
Kovacs, T
Hansen, T
Beky, B
Noyes, RW
Lazar, J
Papp, I
Sari, P
AF Hartman, J. D.
Bhatti, W.
Bakos, G. A.
Bieryla, A.
Kovacs, G.
Latham, D. W.
Csubry, Z.
de Val-Borro, M.
Penev, K.
Buchhave, L. A.
Torres, G.
Howard, A. W.
Marcy, G. W.
Johnson, J. A.
Isaacson, H.
Sato, B.
Boisse, I.
Falco, E.
Everett, M. E.
Szklenar, T.
Fulton, B. J.
Shporer, A.
Kovacs, T.
Hansen, T.
Beky, B.
Noyes, R. W.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-50b, HAT-P-51b, HAT-P-52b, AND HAT-P-53b: THREE TRANSITING HOT
JUPITERS AND A TRANSITING HOT SATURN FROM THE HATNET SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-50, HAT-P-51, HAT-P-52,
HAT-P-53); techniques: photometric; techniques: spectroscopic
ID UNEQUALLY-SPACED DATA; EXTRASOLAR PLANETS; OKAYAMA HIDES; IODINE CELLS;
KEPLER FIELD; BRIGHT STAR; SUBARU HDS; TELESCOPE; ALGORITHM; ORBIT
AB We report the discovery and characterization of four transiting exoplanets by the HATNet survey. The planet HAT-P-50b has a mass of 1.35 M-J and radius of 1.29 R-J, and orbits a bright (V = 11.8 mag) M = 1.27 M-circle dot, R = 1.70 R-circle dot star every P = 3.1220 days. The planet HAT-P-51b has a mass of 0.31 M-J and radius of 1.29 R-J, and orbits a V = 13.4 mag, M = 0.98 M-circle dot, R = 1.04 R. star with a period of P = 4.2180 days. The planet HAT-P-52b has a mass of 0.82M(J) and radius of 1.01 R-J, and orbits a V = 14.1 mag, M = 0.89 M-circle dot, R = 0.89 R-circle dot star with a period of P = 2.7536 days. The planet HAT-P-53b has a mass of 1.48 M-J and radius of 1.32 R-J, and orbits a V = 13.7 mag, M = 1.09 M-circle dot, R = 1.21R. star with a period of P = 1.9616 days. All four planets are consistent with having circular orbits and have masses and radii measured to better than 10% precision. The low stellar jitter and favorable Rp/R circle dot ratio for HAT-P-51 make it a promising target for measuring the Rossiter-McLaughlin effect for a Saturnmass planet.
C1 [Hartman, J. D.; Bhatti, W.; Bakos, G. A.; Csubry, Z.; de Val-Borro, M.; Penev, K.; Kovacs, T.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bieryla, A.; Latham, D. W.; Buchhave, L. A.; Torres, G.; Johnson, J. A.; Falco, E.; Beky, B.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovacs, G.; Kovacs, T.] Konkoly Observ Budapest, Budapest, Hungary.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, L. A.] Natl Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Howard, A. W.; Fulton, B. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Marcy, G. W.; Isaacson, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Sato, B.] Tokyo Inst Technol, Meguro Ku, Tokyo 1528550, Japan.
[Boisse, I.] Aix Marseille Univ, CNRS, UMR 7326, LAM, F-13388 Marseille, France.
[Everett, M. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Szklenar, T.; Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
[Shporer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hansen, T.] ZAH, Landessternwarte, D-69117 Heidelberg, Germany.
RP Hartman, JD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM jhartman@astro.princeton.edu
OI Penev, Kaloyan/0000-0003-4464-1371; Bakos, Gaspar/0000-0001-7204-6727;
Buchhave, Lars A./0000-0003-1605-5666; Hartman,
Joel/0000-0001-8732-6166; Latham, David/0000-0001-9911-7388
FU NASA [NNG04GN74G, NNX08AF23G, NNX13AJ15G, NNX09AB29G, NNX14AF87G,
NNX13AQ62G, NNX14AB83G]; NSF [AST-1108686]; Kepler Mission under NASA
[NCC2-1390]; Robert Martin Ayers Sciences Fund
FX HATNet operations have been funded by NASA grants NNG04GN74G,
NNX08AF23G, and NNX13AJ15G. Follow-up of HATNet targets has been
partially supported through NSF grant AST-1108686. G. A. B, Z. C. and K.
P. acknowledge partial support from NASA grant NNX09AB29G. J. H.
acknowledges support from NASA grant NNX14AF87G. K. P. acknowledges
support from NASA grant NNX13AQ62G. G. T. acknowledges partial support
from NASA grant NNX14AB83G. We acknowledge partial support also from the
Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D.W.L., PI).
Data presented in this paper are based on observations obtained at the
HAT station at the Submillimeter Array of SAO, and the HAT station at
the Fred Lawrence Whipple Observatory of SAO. The authors wish to
acknowledge the very significant cultural role and reverence 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 has made use of Keck
telescope time granted through NOAO (program A245Hr) and NASA (N154Hr,
N130Hr). This research was made possible through the use of the AAVSO
Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers
Sciences Fund.
NR 56
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD DEC
PY 2015
VL 150
IS 6
AR 168
DI 10.1088/0004-6256/150/6/168
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY7KZ
UT WOS:000366588600003
ER
PT J
AU Kessler, R
Marriner, J
Childress, M
Covarrubias, R
D'Andrea, CB
Finley, DA
Fischer, J
Foley, RJ
Goldstein, D
Gupta, RR
Kuehn, K
Marcha, M
Nichol, RC
Papadopoulos, A
Sako, M
Scolnic, D
Smith, M
Sullivan, M
Wester, W
Yuan, F
Abbott, T
Abdalla, FB
Allam, S
Benoit-Levy, A
Bernstein, GM
Bertin, E
Brooks, D
Rosell, AC
Kind, MC
Castander, FJ
Crocce, M
Da Costa, LN
Desai, S
Diehl, HT
Eifler, TF
Neto, AF
Flaugher, B
Frieman, J
Gerdes, DW
Gruen, D
Gruendl, RA
Honscheid, K
James, DJ
Kuropatkin, N
Li, TS
Maia, MAG
Marshall, JL
Martini, P
Miller, CJ
Miquel, R
Nord, B
Ogando, R
Plazas, AA
Reil, K
Romer, AK
Roodman, A
Sanchez, E
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Tarle, G
Thaler, J
Thomas, RC
Tucker, D
Walker, AR
AF Kessler, R.
Marriner, J.
Childress, M.
Covarrubias, R.
D'Andrea, C. B.
Finley, D. A.
Fischer, J.
Foley, R. J.
Goldstein, D.
Gupta, R. R.
Kuehn, K.
Marcha, M.
Nichol, R. C.
Papadopoulos, A.
Sako, M.
Scolnic, D.
Smith, M.
Sullivan, M.
Wester, W.
Yuan, F.
Abbott, T.
Abdalla, F. B.
Allam, S.
Benoit-Levy, A.
Bernstein, G. M.
Bertin, E.
Brooks, D.
Rosell, A. Carnero
Kind, M. Carrasco
Castander, F. J.
Crocce, M.
Da Costa, L. N.
Desai, S.
Diehl, H. T.
Eifler, T. F.
Neto, A. Fausti
Flaugher, B.
Frieman, J.
Gerdes, D. W.
Gruen, D.
Gruendl, R. A.
Honscheid, K.
James, D. J.
Kuropatkin, N.
Li, T. S.
Maia, M. A. G.
Marshall, J. L.
Martini, P.
Miller, C. J.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A. A.
Reil, K.
Romer, A. K.
Roodman, A.
Sanchez, E.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Tarle, G.
Thaler, J.
Thomas, R. C.
Tucker, D.
Walker, A. R.
CA DES Collaboration
TI THE DIFFERENCE IMAGING PIPELINE FOR THE TRANSIENT SEARCH IN THE DARK
ENERGY SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE supernovae: general; techniques: image processing
ID SUPERNOVA LEGACY SURVEY; IA SUPERNOVAE; COSMOLOGICAL CONSTRAINTS;
PHOTOMETRIC REDSHIFTS; LIGHT CURVES; CALIBRATION; SEXTRACTOR; ALGORITHM;
SOFTWARE; CATALOG
AB We describe the operation and performance of the difference imaging pipeline (DiffImg) used to detect transients in deep images from the Dark Energy Survey Supernova program (DES-SN) in its first observing season from 2013 August through 2014 February. DES-SN is a search for transients in which ten 3 deg(2) fields are repeatedly observed in the g, r, i, z passbands with a cadence of about 1 week. The observing strategy has been optimized to measure high-quality light curves and redshifts for thousands of Type Ia supernovae (SNe Ia) with the goal of measuring dark energy parameters. The essential DiffImg functions are to align each search image to a deep reference image, do a pixel-by-pixel subtraction, and then examine the subtracted image for significant positive detections of point-source objects. The vast majority of detections are subtraction artifacts, but after selection requirements and image filtering with an automated scanning program, there are similar to 130 detections per deg(2) per observation in each band, of which only similar to 25% are artifacts. Of the similar to 7500 transients discovered by DES-SN in its first observing season, each requiring a detection on at least two separate nights, Monte Carlo (MC) simulations predict that 27% are expected to be SNe Ia or core-collapse SNe. Another similar to 30% of the transients are artifacts in which a small number of observations satisfy the selection criteria for a single-epoch detection. Spectroscopic analysis shows that most of the remaining transients are AGNs and variable stars. Fake SNe Ia are overlaid onto the images to rigorously evaluate detection efficiencies and to understand the DiffImg performance. The DiffImg efficiency measured with fake SNe agrees well with expectations from a MC simulation that uses analytical calculations of the fluxes and their uncertainties. In our 8 "shallow" fields with single-epoch 50% completeness depth similar to 23.5, the SN Ia efficiency falls to 1/2 at redshift z approximate to 0.7; in our 2 "deep" fields with mag-depth similar to 24.5, the efficiency falls to 1/2 at z approximate to 1.1. A remaining performance issue is that the measured fluxes have additional scatter (beyond Poisson fluctuations) that increases with the host galaxy surface brightness at the transient location. This bright-galaxy issue has minimal impact on the SNe Ia program, but it may lower the efficiency for finding fainter transients on bright galaxies.
C1 [Kessler, R.; Scolnic, D.; Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kessler, R.; Frieman, J.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Marriner, J.; Finley, D. A.; Wester, W.; Allam, S.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Nord, B.; Soares-Santos, M.; Sobreira, F.; Tucker, D.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Childress, M.; Yuan, F.] Australian Natl Univ, ARC Ctr Excellence All sky Astrophys CAASTRO, Canberra, ACT 2611, Australia.
[Childress, M.; Yuan, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia.
[Covarrubias, R.; Kind, M. Carrasco; Gruendl, R. A.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[D'Andrea, C. B.; Nichol, R. C.; Papadopoulos, A.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Fischer, J.; Sako, M.; Bernstein, G. M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Foley, R. J.; Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, R. J.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Goldstein, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Goldstein, D.; Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Gupta, R. R.] Argonne Natl Lab, Lemont, IL 60439 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Marcha, M.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England.
[Smith, M.; Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile.
[Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Bertin, E.] Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France.
[Rosell, A. Carnero; Da Costa, L. N.; Neto, A. Fausti; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinstituc E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Rosell, A. Carnero; Da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observatorio Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Castander, F. J.; Crocce, M.] IEEC CSIC, Fac Ciencias, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Desai, S.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Desai, S.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gerdes, D. W.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gruen, D.] Univ Munich, Univ Sternwarte, Fak Phys, D-81679 Munich, Germany.
[Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain.
RP Kessler, R (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
EM kessler@kicp.uchicago.edu
RI Ogando, Ricardo/A-1747-2010; Sanchez, Eusebio/H-5228-2015; Sobreira,
Flavia/F-4168-2015;
OI Ogando, Ricardo/0000-0003-2120-1154; Sanchez,
Eusebio/0000-0002-9646-8198; Sobreira, Flavia/0000-0002-7822-0658;
Carrasco Kind, Matias/0000-0002-4802-3194; Goldstein,
Daniel/0000-0003-3461-8661; Abdalla, Filipe/0000-0003-2063-4345;
Sullivan, Mark/0000-0001-9053-4820; Tucker, Douglas/0000-0001-7211-5729
FU National Energy Research Scientific Computing Center (NERSC); Office of
Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Australian
Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
[CE110001020]; U.S. Department of Energy; U.S. 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 Dark Energy Survey; National Science
Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274,
FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234];
European Union
FX This research used resources of the National Energy Research Scientific
Computing Center (NERSC), a DOE Office of Science User Facility
supported by the Office of Science of the U.S. Department of Energy
under Contract No. DE-AC02-05CH11231. Part of this research was
conducted by the Australian Research Council Centre of Excellence for
All-sky Astrophysics (CAASTRO), through project number CE110001020.
Funding for the DES Projects has been provided by the U.S. Department of
Energy, the U.S. 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 Dark Energy Survey. The DES data
management system is supported by the National Science Foundation under
Grant Number AST-1138766. 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, some of which include ERDF funds from the European Union.
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 theassociated 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. We are grateful for
the extraordinary contributions of our CTIO colleagues and the DECam
Construction, Commissioning and Science Verification teams in achieving
the excellent instrument and telescope conditions that have made this
work possible. The success of this project also relies critically on the
expertise and dedication of the DES Data Management group.
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ER
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AU Rebull, LM
Stauffer, JR
Cody, AM
Gunther, HM
Hillenbrand, LA
Poppenhaeger, K
Wolk, SJ
Hora, J
Hernandez, J
Bayo, A
Covey, K
Forbrich, J
Gutermuth, R
Morales-Calderon, M
Plavchan, P
Song, I
Bouy, H
Terebey, S
Cuillandre, JC
Allen, LE
AF Rebull, L. M.
Stauffer, J. R.
Cody, A. M.
Guenther, H. M.
Hillenbrand, L. A.
Poppenhaeger, K.
Wolk, S. J.
Hora, J.
Hernandez, J.
Bayo, A.
Covey, K.
Forbrich, J.
Gutermuth, R.
Morales-Calderon, M.
Plavchan, P.
Song, I.
Bouy, H.
Terebey, S.
Cuillandre, J. C.
Allen, L. E.
TI YSOVAR: MID-INFRARED VARIABILITY IN NGC 1333
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: pre-main sequence; stars: protostars;
stars: variables: general
ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; T TAURI STARS;
FRANCE-HAWAII-TELESCOPE; SPITZER-SPACE-TELESCOPE; INFRARED VARIABILITY;
SUBSTELLAR OBJECTS; LIGHT CURVES; CSI 2264; X-RAY
AB As part of the Young Stellar Object VARiability (YSOVAR) program, we monitored NGC 1333 for similar to 35 days at 3.6 and 4.5 mu m using the Spitzer Space Telescope. We report here on the mid-infrared variability of the point sources in the similar to 10' x similar to 20' area centered on 03: 29: 06, +31: 19: 30 (J2000). Out of 701 light curves in either channel, we find 78 variables over the YSOVAR campaign. About half of the members are variable. The variable fraction for the most embedded spectral energy distributions (SEDs) (Class I, flat) is higher than that for less embedded SEDs (Class II), which is in turn higher than the star-like SEDs (Class III). A few objects have amplitudes (10-90th percentile brightness) in [3.6] or [4.5] > 0.2 mag; a more typical amplitude is 0.1-0.15 mag. The largest color change is > 0.2 mag. There are 24 periodic objects, with 40% of them being flat SED class. This may mean that the periodic signal is primarily from the disk, not the photosphere, in those cases. We find 9 variables likely to be "dippers," where texture in the disk occults the central star, and 11 likely to be "bursters," where accretion instabilities create brightness bursts. There are 39 objects that have significant trends in [3.6]-[4.5] color over the campaign, about evenly divided between redder-when-fainter (consistent with extinction variations) and bluer-when-fainter. About a third of the 17 Class 0 and/or jet-driving sources from the literature are variable over the YSOVAR campaign, and a larger fraction (similar to half) are variable between the YSOVAR campaign and the cryogenic-era Spitzer observations (6-7 years), perhaps because it takes time for the envelope to respond to changes in the central source. The NGC 1333 brown dwarfs do not stand out from the stellar light curves in any way except there is a much larger fraction of periodic objects (similar to 60% of variable brown dwarfs are periodic, compared to similar to 30% of the variables overall).
C1 [Rebull, L. M.] CALTECH, Infrared Sci Arch IRSA, IPAC, Pasadena, CA 91125 USA.
[Rebull, L. M.; Stauffer, J. R.; Cody, A. M.] CALTECH, SSC, Pasadena, CA 91125 USA.
[Cody, A. M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guenther, H. M.; Poppenhaeger, K.; Wolk, S. J.; Hora, J.; Forbrich, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Guenther, H. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Hillenbrand, L. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Hernandez, J.] Ctr Invest Astron, Merida 5101, Venezuela.
[Bayo, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bayo, A.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso 5030, Chile.
[Covey, K.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Covey, K.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
[Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria.
[Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Morales-Calderon, M.; Bouy, H.] Ctr Astrobiol INTA CSIC, Dept Astrofis, E-28691 Villanueva De La Canada, Spain.
[Plavchan, P.] CALTECH, NASA Exoplanet Sci Inst NExScI, IPAC, Pasadena, CA 91125 USA.
[Plavchan, P.] Missouri State Univ, Springfield, MO 65897 USA.
[Song, I.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Terebey, S.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA.
[Cuillandre, J. C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ USA.
RP Rebull, LM (reprint author), CALTECH, Infrared Sci Arch IRSA, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM rebull@ipac.caltech.edu
RI Bouy, Herve/H-2913-2012; Morales-Calderon, Maria/C-8384-2017;
OI Bouy, Herve/0000-0002-7084-487X; Morales-Calderon,
Maria/0000-0001-9526-9499; Poppenhaeger, Katja/0000-0003-1231-2194;
Gunther, Hans Moritz/0000-0003-4243-2840; Wolk,
Scott/0000-0002-0826-9261; Rebull, Luisa/0000-0001-6381-515X; Covey,
Kevin/0000-0001-6914-7797
FU National Aeronautics and Space Administration; National Science
Foundation; Proyecto Fondecyt de Iniciacion [11140572]; Ramon y Cajal
fellowship program [RYC-2009-04497]; Spanish grants
[AYA2012-38897-C02-01, AYA2010-21161-C02-02, CDS2006-00070,
PRICITS2009/ESP-1496]
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. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. The research described in this paper was partially carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The scientific results reported in this article are
based in part on data obtained from the Chandra Data Archive including,
observations made by the Chandra X-ray Observatory and published
previously in cited articles. This research has made use of NASA's
Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD
database, operated at CDS, Strasbourg, France. This research has made
use of data products from the Two Micron All-Sky Survey (2MASS), which
is a joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center, funded by the National Aeronautics and
Space Administration and the National Science Foundation. The 2MASS data
are served by the NASA/IPAC Infrared Science Archive, which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
Brevis esse laboro osbcurus fio. (Horace).; A. Bayo acknowledges
financial support from the Proyecto Fondecyt de Iniciacion 11140572.; H.
Bouy is funded by the the Ramon y Cajal fellowship program number
RYC-2009-04497. This research has been funded by Spanish grants
AYA2012-38897-C02-01, AYA2010-21161-C02-02, CDS2006-00070 and
PRICITS2009/ESP-1496. This work used Topcat (Taylor 2005) and Stilts
(Taylor 2006). Based in part on data collected at Subaru Telescope and
obtained from the SMOKA, which is operated by the Astronomy Data Center,
National Astronomical Observatory of Japan. This research used the
facilities of the Canadian Astronomy Data Centre operated by the
National Research Council of Canada with the support of the Canadian
Space Agency. Based on observations obtained with MegaPrime/MegaCam, a
joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii
Telescope (CFHT) which is operated by the National Research Council
(NRC) of Canada, the Institute National des Sciences de l'Univers of the
Centre National de la Recherche Scientifique of France, and the
University of Hawaii.
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AU Rivkin, AS
Thomas, CA
Howell, ES
Emery, JP
AF Rivkin, Andrew S.
Thomas, Cristina A.
Howell, Ellen S.
Emery, Joshua P.
TI THE Ch-CLASS ASTEROIDS: CONNECTING A VISIBLE TAXONOMIC CLASS TO A 3 mu m
BAND SHAPE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE meteorites, meteors, meteoroids; minor planets, asteroids: general;
techniques: spectroscopic
ID SPECTRAL REFLECTANCE PROPERTIES; LOW-ALBEDO ASTEROIDS; MAIN BELT
ASTEROIDS; CARBONACEOUS CHONDRITES; SPECTROSCOPIC SURVEY; AQUEOUS
ALTERATION; OUTER-BELT; PHASE-II; WATER; METEORITES
AB Asteroids belonging to the Ch spectral taxonomic class are defined by the presence of an absorption near 0.7 mu m, which is interpreted as due to Fe-bearing phyllosilicates. Phyllosilicates also cause strong absorptions in the 3 mu m region, as do other hydrated and hydroxylated minerals and H2O ice. Over the past decade, spectral observations have revealed different 3 mu m band shapes in the asteroid population. Although a formal taxonomy is yet to be fully established, the "Pallas-type" spectral group is most consistent with the presence of phyllosilicates. If Ch class and Pallas type are both indicative of phyllosilicates, then all Ch-class asteroids should also be Pallas-type. In order to test this hypothesis, we obtained 42 observations of 36 Ch-class asteroids in the 2 to 4 mu m spectral region. We found that 88% of the spectra have 3 mu m band shapes most consistent with the Pallas-type group. This is the first asteroid class for which such a strong correlation has been found. Because the Ch class is defined by the presence of an absorption near 0.7 mu m, this demonstrates that the 0.7 mu m band serves not only as a proxy for the presence of a band in the 3 mu m region, but specifically for the presence of Pallas-type bands. There is some evidence for a correlation between band depth at 2.95 mu m and absolute magnitude and/or albedo. However, we find only weak correlations between 2.95 mu m band depth and semimajor axis. The connection between band depths in the 0.7 and 3 mu m regions is complex and in need of further investigation.
C1 [Rivkin, Andrew S.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
[Thomas, Cristina A.] NASA, Goddard Space Flight Ctr, New York, NY USA.
[Howell, Ellen S.] USRA, Arecibo Observ, Columbia, PR USA.
[Emery, Joshua P.] Univ Tennessee, Knoxville, TN 37996 USA.
RP Rivkin, AS (reprint author), Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
OI Rivkin, Andrew/0000-0002-9939-9976
FU NASA Planetary Astronomy program [NAG5-13221, NNG05GR60G, NNX09AB45G,
NNX14AJ39G]; NSF [AST-1109855]; NASA NEOO [NNX12AF24G]; NASA
Postdoctoral Program at Goddard Space Flight Center; National Science
Foundation [AST-0838261]
FX A.S.R. gratefully acknowledges consistent support from the NASA
Planetary Astronomy program, including grants NAG5-13221, NNG05GR60G,
NNX09AB45G, and NNX14AJ39G. E.S.H. was partially supported by NSF
AST-1109855 and NASA NEOO NNX12AF24G. C.A.T. was supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administrated by Oak Ridge Associated Universities through a
contract with NASA. This material is based upon work at the Caltech
Submillimeter Observatory, which was operated by the California
Institute of Technology under cooperative agreement with the National
Science Foundation (AST-0838261). We acknowledge the sacred nature of
Mauna Kea to many Hawaiians, and our status as guests who have been
privileged to work there. Many thanks to the stalwart telescope
operators of the IRTF who were instrumental in taking these data through
the years, and to Bobby Bus and Eric Volquardsen for developing the
"ATRAN part" of the data reduction. A.S.R. thanks Ashwin Raghavachari
for his supporting work on the database. This research utilizes spectra
acquired by Takahiro Hiroi with the NASA RELAB facility at Brown
University. Thanks to an anonymous reviewer who we hope is charitably
disposed toward the published paper!
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Palanque-Delabrouille, N
Prakash, A
Paris, I
Yeche, C
Dawson, KS
Bovy, J
Lang, D
Schlegel, DJ
Newman, JA
Petitjean, P
Kneib, JP
Laurent, P
Percival, WJ
Ross, AJ
Seo, HJ
Tinker, JL
Armengaud, E
Brownstein, J
Burtin, E
Cai, Z
Comparat, J
Kasliwal, M
Kulkarni, SR
Laher, R
Levitan, D
McBride, CK
McGreer, ID
Miller, AA
Nugent, P
Ofek, E
Rossi, G
Ruan, J
Schneider, DP
Sesar, B
Streblyanska, F
Surace, J
AF Myers, Adam D.
Palanque-Delabrouille, Nathalie
Prakash, Abhishek
Paris, Isabelle
Yeche, Christophe
Dawson, Kyle S.
Bovy, Jo
Lang, Dustin
Schlegel, David J.
Newman, Jeffrey A.
Petitjean, Patrick
Kneib, Jean-Paul
Laurent, Pierre
Percival, Will J.
Ross, Ashley J.
Seo, Hee-Jong
Tinker, Jeremy L.
Armengaud, Eric
Brownstein, Joel
Burtin, Etienne
Cai, Zheng
Comparat, Johan
Kasliwal, Mansi
Kulkarni, Shrinivas R.
Laher, Russ
Levitan, David
McBride, Cameron K.
McGreer, Ian D.
Miller, Adam A.
Nugent, Peter
Ofek, Eran
Rossi, Graziano
Ruan, John
Schneider, Donald P.
Sesar, Branimir
Streblyanska, Fklina
Surace, Jason
TI THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: QUASAR
TARGET SELECTION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; cosmology: observations; galaxies: distances and redshifts;
galaxies: photometry; methods: data analysis; quasars: general
ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; INTERMEDIATE-REDSHIFT
QUASARS; SURVEY PHOTOMETRIC SYSTEM; FAINT BLUE OBJECTS; BLACK-HOLE
MASSES; 7TH DATA RELEASE; LY-ALPHA FOREST; LUMINOSITY FUNCTION; STELLAR
OBJECTS
AB As part of the Sloan Digital Sky Survey (SDSS) IV the extended Baryon Oscillation Spectroscopic Survey (eBOSS) will improve measurements of the cosmological distance scale by applying the Baryon Acoustic Oscillation (BAO) method to quasar samples. eBOSS will adopt two approaches to target quasars over 7500 deg(2). First, a "CORE" quasar sample will combine the optical selection in ugriz using a likelihood-based routine called XDQSOz, with a mid-IR-optical color cut. eBOSS CORE selection (to g < 22 or r < 22) should return similar to 70 deg(-2) quasars at redshifts 0.9 < z < 2.2 and similar to 7 deg(-2)z > 2.1 quasars. Second, a selection based on variability in multi-epoch imaging from the Palomar Transient Factory should recover an additional similar to 3-4 deg(-2)z > 2.1 quasars to g < 22.5 A linear model of how imaging systematics affect target density recovers the angular distribution of eBOSS CORE quasars over 96.7% (76.7%) of the SDSS north (south) Galactic Cap area. The eBOSS CORE quasar sample should thus be sufficiently dense and homogeneous over 0.9. <. z. <. 2.2 to yield the first few-percent-level BAO constraint near <(z)over bar> similar to 1.5. eBOSS quasars at z > 2.1 will be used to improve BAO measurements in the Ly alpha Forest. Beyond its key cosmological goals, eBOSS should be the next-generation quasar survey, comprising > 500,000 new quasars and >500,000 uniformly selected spectroscopically confirmed 0.9 < z < 2.2 quasars. At the conclusion of eBOSS, the SDSS will have provided unique spectra for more than 800,000 quasars.
C1 [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Palanque-Delabrouille, Nathalie; Yeche, Christophe; Laurent, Pierre; Armengaud, Eric; Burtin, Etienne] CEA, Irfu SPP, Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Prakash, Abhishek; Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Prakash, Abhishek; Newman, Jeffrey A.] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA.
[Paris, Isabelle] Osserv Astron Trieste, INAF, I-34131 Trieste, IT, Italy.
[Dawson, Kyle S.; Brownstein, Joel] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Bovy, Jo] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Lang, Dustin] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA.
[Schlegel, David J.; Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Petitjean, Patrick] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Kneib, Jean-Paul] Ecole Polytech Fed Lausanne, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, Switzerland.
[Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Percival, Will J.; Ross, Ashley J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA.
[Cai, Zheng; McGreer, Ian D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Comparat, Johan] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain.
[Kasliwal, Mansi] Carnegie Inst Sci, Observ, Pasadena, CA 91101 USA.
[Kulkarni, Shrinivas R.; Miller, Adam A.] CALTECH, Pasadena, CA 91125 USA.
[Laher, Russ; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Levitan, David] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[McBride, Cameron K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nugent, Peter] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Ofek, Eran] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea.
[Ruan, John] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Sesar, Branimir] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Streblyanska, Fklina] IAC, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Streblyanska, Fklina] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain.
RP Myers, AD (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
EM amyers14@uwyo.edu
RI EPFL, Physics/O-6514-2016
FU Alexander von Humboldt Foundation at the Max-Planck-Institut fur
Astronomie; NASA-ADAP awards [NNX12AI49G, NNX12AE38G]; NSF [1211112,
1515404]; ERC; National Aeronautics and Space Administration; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of Energy
Office of Science; Center for High-Performance Computing at the
University of Utah
FX We are grateful for insightful discussions about quasar selection
statistics with Joe Hennawi, David Hogg, and Gordon Richards. A.D.M.
acknowledges a generous research fellowship from the Alexander von
Humboldt Foundation at the Max-Planck-Institut fur Astronomie and was
supported in part by NASA-ADAP awards NNX12AI49G and NNX12AE38G and by
NSF awards 1211112 and 1515404. J.P.K. acknowledges support from the ERC
advanced grant LIDA.; 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.; 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 141
TC 16
Z9 16
U1 2
U2 7
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 DEC
PY 2015
VL 221
IS 2
AR 27
DI 10.1088/0067-0049/221/2/27
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY7WV
UT WOS:000366620900005
ER
PT J
AU Kelley, CA
Chanton, JP
Bebout, BM
AF Kelley, Cheryl A.
Chanton, Jeffrey P.
Bebout, Brad M.
TI Rates and pathways of methanogenesis in hypersaline environments as
determined by C-13-labeling
SO BIOGEOCHEMISTRY
LA English
DT Article
DE C-13-labeling; Hypersaline environments; Methane; Stable carbon isotopes
ID CARBON-ISOTOPE FRACTIONATION; METHANE PRODUCTION; MICROBIAL MATS;
METHANOSARCINA-BARKERI; SUBSTRATE LIMITATION; SULFATE REDUCTION;
MARINE-SEDIMENTS; TIBETAN PLATEAU; ORGANIC-MATTER; ZOIGE WETLAND
AB Rates and pathways of methane production were determined from photosynthetic soft microbial mats and gypsum-encrusted endoevaporites collected in hypersaline environments from California, Mexico and Chile, as well as an organic-rich mud from a pond in the El Tatio volcanic fields, Chile. Samples (mud, soft mats and endoevaporites) were incubated anaerobically with deoxygenated site water, and the increase in methane concentration through time in the headspaces of the incubation vials was used to determine methane production rates. To ascertain the substrates used by the methanogens, C-13-labeled methylamines, methanol, dimethylsulfide, acetate or bicarbonate were added to the incubations (one substrate per vial) and the stable isotopic composition of the resulting methane was measured. The vials amended with C-13-labeled methylamines produced the most C-13-enriched methane, generally followed by the C-13-labeled methanol-amended vials. The stable isotope data and the methane production rates were used to determine first order rate constants for each of the substrates at each of the sites. Estimates of individual substrate use revealed that the methylamines produced 55-92 % of the methane generated, while methanol was responsible for another 8-40 %.
C1 [Kelley, Cheryl A.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
[Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Bebout, Brad M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
RP Kelley, CA (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
EM kelleyc@missouri.edu
FU NASA Exobiology program
FX Funding by the NASA Exobiology program is gratefully acknowledged. We
would also like to thank Angela Detweiler, Adrienne Frisbee, Amanda
Tazaz, Tyler Mauney, Jennifer Poole, Brooke Nicholson, Claire Beaudoin,
and Alfonso Davila, as well as our many colleagues in Mexico and Chile,
for help in the field and laboratory. We are also appreciative of the
access to the field sites provided by Exportadora de Sal, S.A. de C.V
and the U.S. Fish and Wildlife Service. Neal Blair is thanked for his
thoughtful comments on an earlier version of the manuscript.
NR 44
TC 0
Z9 0
U1 9
U2 22
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
EI 1573-515X
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD DEC
PY 2015
VL 126
IS 3
BP 329
EP 341
DI 10.1007/s10533-015-0161-9
PG 13
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA CY8AT
UT WOS:000366631500006
ER
PT J
AU Balazs, GH
Van Houtan, KS
Hargrove, SA
Brunson, SM
Murakawa, SKK
AF Balazs, George H.
Van Houtan, Kyle S.
Hargrove, Stacy A.
Brunson, Shandell M.
Murakawa, Shawn K. K.
TI A Review of the Demographic Features of Hawaiian Green Turtles (Chelonia
mydas)
SO CHELONIAN CONSERVATION AND BIOLOGY
LA English
DT Review
DE Reptilia; Testudines; Northwestern Hawaiian Islands; French Frigate
Shoals; nesting biology; population monitoring
ID SEA-TURTLES; ARCHIPELAGO; RECOVERY; ISLANDS; GROWTH
AB This review summarizes all existing data and knowledge of the demographic variables and their stochasticity of Hawaiian green turtles. The population numbers roughly 4000 breeding females today, having rebounded from its near extinction in the early 1970s, with most of the nesting restricted to French Frigate Shoals in the remote and geologically ancient Northwestern Hawaiian Islands. A timeline is provided of the scientific monitoring for this population and associated data streams relating to morphometrics, maturity, nest dynamics, sex ratio, as well as population growth and viability.
C1 [Balazs, George H.; Van Houtan, Kyle S.; Brunson, Shandell M.; Murakawa, Shawn K. K.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
[Van Houtan, Kyle S.] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA.
[Hargrove, Stacy A.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL 33149 USA.
RP Balazs, GH (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM george.balazs@noaa.gov; kyle.vanhoutan@noaa.gov;
stacy.hargrove@noaa.gov; shandell.brunson@noaa.gov;
shawn.murakawa@noaa.gov
OI Van Houtan, Kyle/0000-0001-5725-1773
NR 51
TC 3
Z9 4
U1 7
U2 25
PU CHELONIAN RESEARCH FOUNDATION
PI LUNENBURG
PA 168 GOODRICH ST., LUNENBURG, MA USA
SN 1071-8443
EI 1943-3956
J9 CHELONIAN CONSERV BI
JI Chelonian Conserv. Biol.
PD DEC
PY 2015
VL 14
IS 2
BP 119
EP 129
PG 11
WC Zoology
SC Zoology
GA CY9YK
UT WOS:000366762100001
ER
PT J
AU Jaroszynski, A
Jaroszynska, A
Siebert, J
Dabrowski, W
Niedziaek, J
Bednarek-Skublewska, A
Zapolski, T
Wysokinski, A
Zaluska, W
Ksiazek, A
Schlegel, TT
AF Jaroszynski, Andrzej
Jaroszynska, Anna
Siebert, Janusz
Dabrowski, Wojciech
Niedziaek, Jarosaw
Bednarek-Skublewska, Anna
Zapolski, Tomasz
Wysokinski, Andrzej
Zaluska, Wojciech
Ksiazek, Andrzej
Schlegel, Todd T.
TI The prognostic value of positive T-wave in lead aVR in hemodialysis
patients
SO CLINICAL AND EXPERIMENTAL NEPHROLOGY
LA English
DT Article
DE Electrocardiogram; End-stage renal disease; T-wave amplitude; Lead aVR;
Cardiovascular mortality; Sudden cardiac death
ID ACUTE MYOCARDIAL-INFARCTION; CHRONIC KIDNEY-DISEASE; ST-SEGMENT
ELEVATION; SUDDEN CARDIAC DEATH; CARDIOVASCULAR MORTALITY;
ELECTROCARDIOGRAPHIC ABNORMALITIES; HEART-FAILURE; LEFT MAIN; RISK;
AMPLITUDE
AB Background Given that cardiac disease is the leading cause of mortality in hemodialysis (HD) patients, identification of patients at risk for cardiac mortality is crucial. The aim of this study was to determine if positive T-wave amplitude in lead aVR (TaVR) was predictive of cardiovascular (CV) mortality and sudden cardiac death (SCD) in a group of HD patients.
Methods and resultsAfter exclusion, 223 HD patients were prospectively followed-up for 25.43 +/- A 3.56 months. Patients were divided into TaVR negative (n = 186) and TaVR positive (n = 37) groups. Myocardial infarction, diabetes and beta-blocker therapy were more frequent in positive TaVR patients. Patients with upright TaVR were older, had higher left ventricular mass index, lower ejection fraction, higher calcium x phosphate product, higher troponin T level, higher prevalence of ST-T abnormalities, and increased width of QRS complex and QT interval, compared with patients with negative TaVR. A Kaplan-Meier analysis showed that the cumulative incidences of CV mortality as well as SCD were higher in patients with positive TaVR compared with those with negative TaVR (log-rank, p < 0.001 in both cases). A multivariate analysis selected age [hazard ratio (HR) 1.71, p < 0.001], heart rate (HR 1.42, p = 0.016), and positive TaVR (HR 2.21, p = 0.001) as well as age (HR 1.88, p < 0.001), and positive TaVR (HR 1.53, p = 0.014) as independent predictors of CV mortality and SCD, respectively.
ConclusionIn HD patients, positive TaVR is an independent and powerful predictor of CV mortality as well as SCD. This simple ECG parameter provides additional information beyond what is available with other known traditional risk factors and allows the identification of patients most at risk of CV events.
C1 [Jaroszynski, Andrzej; Niedziaek, Jarosaw] Med Univ Lublin, Dept Family Med, PL-20081 Lublin, Poland.
[Jaroszynska, Anna; Zapolski, Tomasz; Wysokinski, Andrzej] Med Univ Lublin, Dept Cardiol, PL-20081 Lublin, Poland.
[Siebert, Janusz] Med Univ Gdansk, Univ Ctr Cardiol, Dept Family Med, Gdansk, Poland.
[Dabrowski, Wojciech] Med Univ Lublin, Dept Anesthesiol & Intens Care, Lublin, Poland.
[Bednarek-Skublewska, Anna; Zaluska, Wojciech; Ksiazek, Andrzej] Med Univ Lublin, Dept Nephrol, Lublin, Poland.
[Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Jaroszynski, A (reprint author), Med Univ Lublin, Dept Family Med, Staszica 11, PL-20081 Lublin, Poland.
EM jaroszynskiaj@interia.pl
NR 29
TC 2
Z9 2
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1342-1751
EI 1437-7799
J9 CLIN EXP NEPHROL
JI Clin. Exp. Nephrol.
PD DEC
PY 2015
VL 19
IS 6
BP 1157
EP 1164
DI 10.1007/s10157-015-1100-8
PG 8
WC Urology & Nephrology
SC Urology & Nephrology
GA CY7YS
UT WOS:000366626000021
PM 25724127
ER
PT J
AU Shuler, RL
AF Shuler, Robert L.
TI Porting and Scaling Strategies for Nanoscale CMOS RHBD
SO IEEE TRANSACTIONS ON CIRCUITS AND SYSTEMS I-REGULAR PAPERS
LA English
DT Article
DE Aerospace components; CMOS integrated circuits; fault tolerance;
redundancy; space technology
ID SINGLE-EVENT UPSETS; FLIP-FLOPS; DUAL-RAIL; NM CMOS; SEU; DESIGN; LATCH
AB Techniques are described for minimizing the number of cells in a digital logic library, scaling and porting the cells to process nodes that do not nominally support scaling, and increasing the separation of critical node pairs without unduly disrupting the design process. A new compact modular 10T compact continuously-voting latch cell reduces circuitry to conventional latch sizes, at less power, allowing modular redundancy to approach theoretical efficiency limits. The result is allows investment in low volume designs, such as but not limited to radiation hardened by design (RHBD) applications for mission critical components, to provide returns over decades-long time periods.
C1 [Shuler, Robert L.] NASA, Houston, TX 77058 USA.
RP Shuler, RL (reprint author), NASA, Houston, TX 77058 USA.
EM robert.l.shuler@nasa.gov
OI Shuler, Robert/0000-0002-6129-6867
NR 22
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1549-8328
EI 1558-0806
J9 IEEE T CIRCUITS-I
JI IEEE Trans. Circuits Syst. I-Regul. Pap.
PD DEC
PY 2015
VL 62
IS 12
BP 2856
EP 2863
DI 10.1109/TCSI.2015.2495779
PG 8
WC Engineering, Electrical & Electronic
SC Engineering
GA CZ1AA
UT WOS:000366836800008
ER
PT J
AU Quick, MG
Krider, EP
AF Quick, Mason G.
Krider, E. Philip
TI Optical emission and peak electromagnetic power radiated by negative
return strokes in rocket-triggered lightning
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Lightning Return stroke; Optical emission; Poynting power; Radiative
fraction
ID EASTERN NEW-YORK; PERFORMANCE EVALUATION; DETECTION NETWORK; DISCHARGES;
CURRENTS; FIELDS; DYNAMICS; ANTENNA; FLORIDA
AB Calibrated measurements of the optical radiation produced by negative return strokes in rocket-triggered lightning (RTL) have been made in the visible and near infrared (VNIR) spectral region in correlation with currents measured at the channel base. Using a simple transmission-line model, the currents have been used to estimate the peak electromagnetic (EM) fields and Poynting power that are radiated in the time-domain (i.e. from about 1 kHz to 3 MHz). The results show that the optical power radiated by RTL at the time of the peak current has a mean and standard deviation of 130 +/- 120 MW, a value that is only about 5% of the Poynting power that is radiated into the upper half-space at that time. These results are in good agreement with similar measurements made on the subsequent return strokes in natural lightning that remain in a pre-existing channel. Our methods and assumptions are similar to those of (Gun and Krider, 1983; Krider and Guo, 1983; Quick and Krider, 2013). (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Quick, Mason G.; Krider, E. Philip] Univ Arizona, Inst Atmospher Phys, Tucson, AZ 85721 USA.
RP Quick, MG (reprint author), NASA MSFC, NASA NSSTC ZP11, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM mgquick@atmo.arizona.edu
FU DARPA NIMBUS program through the University of Florida [DARPA-BAA-10-18]
FX We are grateful to M. P. Lesser and R. Tucker in the Imaging Technology
Laboratory at the University of Arizona for assistance with the sensor
calibrations; to R. C. Noggle for assistance with the electronics and
construction of the sensors; to K. L. Cummins and C. D. Weidman for a
number of helpful discussions; to M. A. Uman, D. M. Jordan, J. D. Hill,
and numerous others at the ICLRT for their assistance with the
experiment and data acquisition. This work has been supported in part by
the DARPA NIMBUS program through the University of Florida under
DARPA-BAA-10-18.
NR 39
TC 0
Z9 0
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD DEC
PY 2015
VL 136
SI SI
BP 80
EP 85
PN A
PG 6
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA CZ0JA
UT WOS:000366789900012
ER
PT J
AU Remillard, J
Tselioudis, G
AF Remillard, Jasmine
Tselioudis, George
TI Cloud Regime Variability over the Azores and Its Application to Climate
Model Evaluation
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Atm; Ocean Structure; Phenomena; Cumulus clouds; Stratiform clouds;
Physical Meteorology and Climatology; Clouds; Observational techniques
and algorithms; Climate classification; regimes; Models and modeling;
Climate models
ID TROPICAL WESTERN PACIFIC; SOUTHERN-OCEAN; SURFACE OBSERVATIONS;
RADIATION BIASES; WEATHER STATES; STRATOCUMULUS; PRECIPITATION;
SATELLITE; CYCLONES; GCM
AB From its location on the subtropics-midlatitude boundary, the Azores is influenced by both the subtropical high pressure and the midlatitude baroclinic storm regimes and therefore experiences a wide range of cloud structures, from fair-weather scenes to stratocumulus sheets and deep convective systems. This work combines three types of datasets to study cloud variability in the Azores: a satellite analysis of cloud regimes, a reanalysis characterization of storminess, and a 19-month field campaign that occurred on Graciosa Island. Combined analysis of the three datasets provides a detailed picture of cloud variability and the respective dynamic influences, with emphasis on low clouds that constitute a major uncertainty source in climate model simulations. The satellite cloud regime analysis shows that the Azores cloud distribution is similar to the mean global distribution and can therefore be used to evaluate cloud simulation in global models. Regime analysis of low clouds shows that stratocumulus decks occur under the influence of the Azores high pressure system, while shallow cumulus clouds are sustained by cold-air outbreaks, as revealed by their preference for postfrontal environments and northwesterly flows. An evaluation of climate model cloud regimes from phase 5 of CMIP (CMIP5) over the Azores shows that all models severely underpredict shallow cumulus clouds, while most models also underpredict the occurrence of stratocumulus cloud decks. It is demonstrated that the regime analysis can assist in the selection of case studies representing specific climatological cloud distributions. With all the tools now in place, a methodology is suggested to better understand cloud-dynamics interactions and attempt to explain and correct climate model cloud deficiencies.
C1 Columbia Univ, New York, NY USA.
NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Remillard, J (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, 100 Nicolls Rd, Stony Brook, NY 11794 USA.
EM jasmine.remillard@mail.mcgill.ca
FU DOE Atmospheric Systems Research (ASR) Program [DE-SC0006712]
FX The authors acknowledge the support of the DOE Atmospheric Systems
Research (ASR) Program, under Grant DE-SC0006712.
NR 38
TC 2
Z9 2
U1 3
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD DEC
PY 2015
VL 28
IS 24
BP 9707
EP 9720
DI 10.1175/JCLI-D-15-0066.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CY9IO
UT WOS:000366720800010
ER
PT J
AU Ray, JDM
Sethi, SA
Eiler, JH
Joyce, JE
AF Ray, James D. M.
Sethi, Suresh A.
Eiler, John H.
Joyce, John E.
TI Prespawning Movements and Spawning Distribution of Sockeye Salmon in an
Urbanizing Alaskan Lake
SO JOURNAL OF FISH AND WILDLIFE MANAGEMENT
LA English
DT Article
DE lake habitat; land use; movement; sockeye salmon; spawning distribution;
staging behavior
ID ONCORHYNCHUS-NERKA; BRITISH-COLUMBIA; DIFFERENTIATION; BEHAVIOR; RIVER
AB The efficacy of fish habitat conservation in land planning processes in Alaska is often constrained by the extent of current knowledge of fish distributions and habitat use. In response to requests for information from land and salmon resource management stakeholders regarding Auke Lake sockeye salmon (Oncorhynchus nerka) status and life history, we examined the prespawning movements and spawning distribution of adult sockeye salmon to provide ecological information needed for Auke Lake watershed management. We used radiotelemetry to track the movements of 80 fish in the Auke Lake watershed during 2012. The prespawning distribution of the fish was not random, indicating five spatially and temporally distinct high-use staging areas within the lake. The Auke Lake sockeye salmon population was dominated by stream-spawning fish (98.5%), with minimal lakeshore spawning (1.5%) observed in association with a small intermittent tributary of the lake. The prespawning distribution patterns identified in this study corroborate observations from Auke Lake 20 y ago, indicating consistent habitat use patterns by sockeye salmon in the lake. Telemetry data also indicate 12% of sockeye salmon expired in Auke Lake without spawning and that 14% of stream-spawning fish were preyed upon by black bear (Usrus americanus). The prespawning and spawning behavior by Auke Lake sockeye salmon suggest that discrete lake staging areas and stream spawning beds are important candidate habitats for protection during the land planning process for shoreline development surrounding the lake.
C1 [Ray, James D. M.] Calif Dept Fish & Wildlife, Aquaculture & Bay Management, Eureka, CA 95501 USA.
[Sethi, Suresh A.] US Fish & Wildlife Serv, Conservat Genet Lab, Anchorage, AK 99503 USA.
[Eiler, John H.; Joyce, John E.] Natl Marine Fisheries Serv, Ted Stevens Marine Res Inst, Juneau, AK 99801 USA.
RP Ray, JDM (reprint author), Calif Dept Fish & Wildlife, Aquaculture & Bay Management, 619 Second St, Eureka, CA 95501 USA.
EM James.Ray@wildlife.ca.gov
FU Alaska Sustainable Salmon Fund
FX This project was funded under the Alaska Sustainable Salmon Fund with
additional contributions from the Alaska Department of Transportation
and Public Facilities.
NR 41
TC 0
Z9 0
U1 4
U2 10
PU U S FISH & WILDLIFE SERVICE
PI SHEPHERDSTOWN
PA NATL CONSERVATION TRAINING CENTER, CONSERVATION LIBRARY, 698
CONSERVATION WAY, SHEPHERDSTOWN, WV 25443 USA
SN 1944-687X
J9 J FISH WILDL MANAG
JI J. Fish Wildl. Manag.
PD DEC
PY 2015
VL 6
IS 2
BP 472
EP 485
DI 10.3996/112014-JFWM-083
PG 14
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CY8TT
UT WOS:000366681900020
ER
PT J
AU Roth, DJ
Rauser, RW
AF Roth, D. J.
Rauser, R. W.
TI The Effect of Experiment Variabies on Industrial X-ray Micro-computed
Tomography Sensitivity
SO MATERIALS EVALUATION
LA English
DT Article
DE nondestructive testing; NDT; computed tomography; imaging; X-ray;
metallic components; thin wall inspection; signal-to-noise ratio
AB A study was performed on the effect of experimental variables on radiographic sensitivity (image quality) in X-ray micro-computed tomography images for a high-density thin wall metallic cylinder containing micro-electrical discharge machining holes. Image quality was evaluated in terms of signal-to-noise ratio (SNR) discontinuity detectability, and feature sharpness. The variables included: day-to-day reproducibility, current, integration time, voltage, filtering, number of frame averages, number of projection views, beam width, effective object radius, binning, orientation of sample, acquisition angle range (180 to 3609, and directional versus transmission tube. This paper presents a tabular summary of the findings. In most, but not all cases, SNR, discontinuity detectability, and feature sharpness changed as expected/predicted with changing X-ray parameters.
C1 [Roth, D. J.] NASA Glenn Res Ctr, ASNT NDT Level 3, Cleveland, OH 44135 USA.
[Rauser, R. W.] Univ Toledo, Toledo, OH 43606 USA.
RP Roth, DJ (reprint author), NASA Glenn Res Ctr, ASNT NDT Level 3, Cleveland, OH 44135 USA.
NR 10
TC 1
Z9 1
U1 3
U2 6
PU AMER SOC NONDESTRUCTIVE TEST
PI COLUMBUS
PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA
SN 0025-5327
J9 MATER EVAL
JI Mater. Eval.
PD DEC
PY 2015
VL 73
IS 12
BP 1577
EP 1584
PG 8
WC Materials Science, Characterization & Testing
SC Materials Science
GA CY2IC
UT WOS:000366231000006
ER
PT J
AU Little, CM
Horton, RM
Kopp, RE
Oppenheimer, M
Vecchi, GA
Villarini, G
AF Little, Christopher M.
Horton, Radley M.
Kopp, Robert E.
Oppenheimer, Michael
Vecchi, Gabriel A.
Villarini, Gabriele
TI Joint projections of US East Coast sea level and storm surge
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID DISSIPATION INDEX PDI; CYCLONE ENERGY ACE; TROPICAL CYCLONES; POWER
DISSIPATION; HURRICANE ACTIVITY; CLIMATE MODELS; UNITED-STATES; CMIP5
MODELS; RISE; VARIABILITY
AB Future coastal flood risk will be strongly influenced by sea-level rise (SLR) and changes in the frequency and intensity of tropical cyclones. These two factors are generally considered independently. Here, we assess twenty-first century changes in the coastal hazard for the US East Coast using a flood index (FI) that accounts for changes in flood duration and magnitude driven by SLR and changes in power dissipation index (PDI, an integrated measure of tropical cyclone intensity, frequency and duration). Sea-level rise and PDI are derived from representative concentration pathway (RCP) simulations of 15 atmosphere-ocean general circulation models (AOGCMs). By 2080-2099, projected changes in the FI relative to 1986-2005 are substantial and positively skewed: a 10th-90th percentile range 4-75 times higher for RCP 2.6 and 35-350 times higher for RCP 8.5. High-end FI projections are driven by three AOGCMs that project the largest increases in SLR, PDI and upper ocean temperatures. Changes in PDI are particularly influential if their intra-model correlation with SLR is included, increasing the RCP 8.5 90th percentile FI by a further 25%. Sea-level rise from other, possibly correlated, climate processes (for example, ice sheet and glacier mass changes) will further increase coastal flood risk and should be accounted for in comprehensive assessments.
C1 [Little, Christopher M.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Horton, Radley M.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Horton, Radley M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Kopp, Robert E.] Rutgers State Univ, Rutgers Energy Inst, Dept Earth & Planetary Sci, Piscataway, NJ 08854 USA.
[Kopp, Robert E.] Rutgers State Univ, Inst Earth Ocean & Atmospher Sci, Piscataway, NJ 08854 USA.
[Oppenheimer, Michael] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA.
[Oppenheimer, Michael] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA.
[Vecchi, Gabriel A.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Villarini, Gabriele] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA 52212 USA.
RP Little, CM (reprint author), Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
EM clittle@aer.com
RI Vecchi, Gabriel/A-2413-2008; Villarini, Gabriele/F-8069-2016;
OI Vecchi, Gabriel/0000-0002-5085-224X; Villarini,
Gabriele/0000-0001-9566-2370; Kopp, Robert/0000-0003-4016-9428
FU Carbon Mitigation Initiative in the Princeton Environmental Institute;
New Jersey Sea Grant under NOAA [6410-0012, NA11OAR4310101]; USACE
Institute for Water Resources
FX C.M.L. is grateful for inspiration from the New York City Panel on
Climate Change and the Structures of Coastal Resilience project
(http://www.structuresofcoastalresilience.org), discussions with R.
Ponte, C. Piecuch and K. Quinn, and financial support from the Carbon
Mitigation Initiative in the Princeton Environmental Institute. The NOAA
Geophysical Fluid Dynamics Laboratory provided data and analysis tools.
R.E.K.'s contribution to this project was supported by New Jersey Sea
Grant project 6410-0012 (under NOAA grant NA11OAR4310101). G.V.
acknowledges financial support from the USACE Institute for Water
Resources. We acknowledge the World Climate Research Programme's Working
Group on Coupled Modeling, which is responsible for CMIP, and we thank
the climate modelling groups (listed in Supplementary Tables 1 and 2)
for producing and making available their model output. The US Department
of Energy's Program for Climate Model Diagnosis and Intercomparison
provides coordinating support for CMIP and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals.
NR 55
TC 12
Z9 12
U1 8
U2 30
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD DEC
PY 2015
VL 5
IS 12
BP 1114
EP +
DI 10.1038/NCLIMATE2801
PG 8
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CY4UA
UT WOS:000366402900023
ER
PT J
AU Huffman, W
Thompson, DR
Bue, B
Castillo-Rogez, J
Boland, J
AF Huffman, W.
Thompson, D. R.
Bue, B.
Castillo-Rogez, J.
Boland, J.
TI Autonomous Onboard Point Source Detection by Small Exploration
Spacecraft
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID COSMIC-RAY REJECTION; NAVIGATION
AB Small spacecraft platforms are a promising low-cost approach to accelerate exploration of small bodies, addressing the space community's interest in origin science, planetary resources, and planetary defense. However, they can be challenging platforms for detecting and imaging low brightness targets. Difficulties include constrained bandwidth, which limits the volume of data that can be downlinked; attitude instability, which limits exposure time; small instrument apertures, which reduce sensitivity; and cosmic ray contamination, which creates illusory sources. Mission designers can address all these problems simultaneously by shifting image analysis across the communications gap. Spacecraft can use onboard data analysis to detect sources directly, or downlink parsimonious summary products for detection on the ground. One promising approach is to acquire stacks of short consecutive exposures, and then coregister and coadd them onboard. This work analyzes a coaddition algorithm that is designed to be robust against small spacecraft challenges. We evaluate factors affecting performance, such as attitude control and camera noise systematics, in regimes typical of small spacecraft missions. We motivate the algorithm design by considering its application to NEAScout, a mission representing a new generation of small (sub-50kg) exploration spacecraft having very small instrument apertures and data rates below 1kbytes(-1). Here, onboard analysis allows detection and rendezvous with far smaller and fainter objects, dramatically reducing the cost and complexity of primitive bodies exploration.
C1 [Huffman, W.; Thompson, D. R.; Bue, B.; Castillo-Rogez, J.; Boland, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Huffman, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM william.c.huffman@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 32
TC 0
Z9 0
U1 2
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD DEC
PY 2015
VL 127
IS 958
BP 1279
EP 1291
DI 10.1086/684172
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY7YE
UT WOS:000366624400008
ER
PT J
AU Currie, T
Cloutier, R
Brittain, S
Grady, C
Burrows, A
Muto, T
Kenyon, SJ
Kuchner, MJ
AF Currie, Thayne
Cloutier, Ryan
Brittain, Sean
Grady, Carol
Burrows, Adam
Muto, Takayuki
Kenyon, Scott J.
Kuchner, Marc J.
TI RESOLVING THE HD 100546 PROTOPLANETARY SYSTEM WITH THE GEMINI PLANET
IMAGER: EVIDENCE FOR MULTIPLE FORMING, ACCRETING PLANETS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: early-type; stars: individual (HD 100546)
ID ORBITING HR 8799; MASS COMPANION; BROWN DWARFS; DISK; CONFIRMATION;
SPECTROSCOPY; HD-100546; LIGHT; DUST
AB We report Gemini Planet Imager H-band high-contrast imaging/integral field spectroscopy and polarimetry of the HD 100546, a 10 Myr old early-type star recently confirmed to host a thermal infrared (IR) bright (super-)Jovian protoplanet at wide separation, HD 100546 b. We resolve the inner disk cavity in polarized light, recover the thermal IR-bright arm, and identify one additional spiral arm. We easily recover HD 100546 b and show that much of its emission plausibly originates from an unresolved point source. The point-source component of HD 100546 b has extremely red IR colors compared to field brown dwarfs, qualitatively similar to young cloudy super-Jovian planets; however, these colors may instead indicate that HD 100546 b is still accreting material from a circumplanetary disk. Additionally, we identify a second point-source-like peak at r(proj) similar to 14 AU, located just interior to or at the inner disk wall consistent with being a < 10-20 M-J candidate second protoplanet-"HD 100546 c"-and lying within a weakly polarized region of the disk but along an extension of the thermal IR-bright spiral arm. Alternatively, it is equally plausible that this feature is a weakly polarized but locally bright region of the inner disk wall. Astrometric monitoring of this feature over the next 2 years and emission line measurements could confirm its status as a protoplanet, rotating disk hot spot that is possibly a signpost of a protoplanet, or a stationary emission source from within the disk.
C1 [Currie, Thayne] Natl Astron Observ Japan, Subaru Telescope, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Cloutier, Ryan] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Cloutier, Ryan] Univ Toronto, Ctr Planetary Sci, Toronto, ON, Canada.
[Cloutier, Ryan] Univ Montreal, Inst Rech Exoplanetes, Montreal, PQ, Canada.
[Brittain, Sean] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Grady, Carol; Kuchner, Marc J.] NASA Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD USA.
[Grady, Carol] Eureka Sci, Oakland, CA USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Tokyo, Japan.
[Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Currie, T (reprint author), Natl Astron Observ Japan, Subaru Telescope, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
OI Kenyon, Scott/0000-0003-0214-609X
FU NASA Origins of Solar Systems program [NNG13PB64P]
FX We thank Gijs Mulders, Wladimir Lyra, Nienke van der Marel, and the
anonymous referee for helpful comments. This work is supported through
NASA Origins of Solar Systems program NNG13PB64P.
NR 37
TC 12
Z9 12
U1 2
U2 6
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 DEC 1
PY 2015
VL 814
IS 2
AR L27
DI 10.1088/2041-8205/814/2/L27
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY0RA
UT WOS:000366112000010
ER
PT J
AU Mingarelli, CMF
Levin, J
Lazio, TJW
AF Mingarelli, Chiara M. F.
Levin, Janna
Lazio, T. Joseph W.
TI FAST RADIO BURSTS AND RADIO TRANSIENTS FROM BLACK HOLE BATTERIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; gravitation; gravitational waves; pulsars: general;
stars: neutron
ID NEUTRON-STAR MERGERS; PULSARS; POPULATIONS; EVOLUTION; ORIGIN
AB Most black holes (BHs) will absorb a neutron star (NS) companion fully intact without tidal disruption, suggesting the pair will remain dark to telescopes. Even without tidal disruption, electromagnetic (EM) luminosity is generated from the battery phase of the binary when the BH interacts with the NS magnetic field. Originally, the luminosity was expected to be in high-energy X-rays or gamma-rays, however, we conjecture that some of the battery power is emitted in the radio bandwidth. While the luminosity and timescale are suggestive of fast radio bursts (FRBs; millisecond-scale radio transients) NS-BH coalescence rates are too low to make these a primary FRB source. Instead, we propose that the transients form a FRB sub-population, distinguishable by a double peak with a precursor. The rapid ramp-up in luminosity manifests as a precursor to the burst which is 20%-80% as luminous given 0.5 ms timing resolution. The main burst arises from the peak luminosity before the merger. The post-merger burst follows from the NS magnetic field migration to the BH, causing a shock. NS-BH pairs are especially desirable for ground-based gravitational wave (GW) observatories since the pair might not otherwise be detected, with EM counterparts greatly augmenting the scientific leverage beyond the GW signal. The EM signal's ability to break degeneracies in the parameters encoded in the GW and probe the NS magnetic field strength is quite valuable, yielding insights into open problems in NS magnetic field decay.
C1 [Mingarelli, Chiara M. F.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Mingarelli, Chiara M. F.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
[Levin, Janna] Columbia Univ, ISCAP, New York, NY 10027 USA.
[Levin, Janna] Barnard Coll, New York, NY 10027 USA.
[Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mingarelli, CMF (reprint author), CALTECH, TAPIR, MC 350-17, Pasadena, CA 91125 USA.
FU Marie Curie International Outgoing Fellowship within the European Union
Seventh Framework Programme; Tow Foundation; Guggenheim Fellowship
FX We thank the referee, M. Vallisneri, and S. Nissanke for carefully
reading the manuscript. We acknowledge valuable discussions with S.
McWilliams, M. Kasliwal, D. Tsang, A. Lommen, F. Pannarale, S. Taylor,
J. Ellis, J. Bell-Burnell, and P. Goldreich. C.M.F.M. was supported by a
Marie Curie International Outgoing Fellowship within the European Union
Seventh Framework Programme. J.L. thanks the Tow Foundation for their
support. J.L. was also supported by a Guggenheim Fellowship. Part of
this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. An ipython notebook which
reproduces our results is available.
https://github.com/ChiaraMingarelli.
NR 45
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Z9 12
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 DEC 1
PY 2015
VL 814
IS 2
DI 10.1088/2041-8205/814/2/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY0RA
UT WOS:000366112000003
ER
PT J
AU Lorenz, RD
Kedar, S
Murdoch, N
Lognonne, P
Kawamura, T
Mimoun, D
Banerdt, WB
AF Lorenz, Ralph D.
Kedar, Sharon
Murdoch, Naomi
Lognonne, Philippe
Kawamura, Taichi
Mimoun, David
Banerdt, W. Bruce
TI Seismometer Detection of Dust Devil Vortices by Ground Tilt
SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA
LA English
DT Article
ID ATMOSPHERIC-PRESSURE CHANGES; PLANETARY SEISMOLOGY; EARTH; FREQUENCY;
RECORDS; LOGGER; NOISE; FIELD
AB We report seismic signals on a desert playa caused by convective vortices and dust devils. The long-period (10-100 s) signatures, with tilts of similar to 10(-7) radians, are correlated with the presence of vortices, detected with nearby sensors as sharp temporary pressure drops (0.2-1 mbar) and solar obscuration by dust. We show that the shape and amplitude of the signals, manifesting primarily as horizontal accelerations, can be modeled approximately with a simple quasi-static point-load model of the negative pressure field associated with the vortices acting on the ground as an elastic half-space. We suggest the load imposed by a dust devil of diameter D and core pressure Delta P-o is similar to(pi/2)Delta PoD2, or for a typical terrestrial dust devil of 5 m diameter and 2 mbar, about the weight of a small car. The tilt depends on the inverse square of distance and on the elastic properties of the ground, and the large signals we observe are in part due to the relatively soft playa sediment and the shallow installation of the instrument. Ground tilt may be a particularly sensitive means of detecting dust devils. The simple point-load model fails for large dust devils at short ranges, but more elaborate models incorporating the work of Sorrells (1971) may explain some of the more complex features in such cases, taking the vortex winds and ground velocity into account. We discuss some implications for the InSight mission to Mars.
C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Kedar, Sharon; Banerdt, W. Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Murdoch, Naomi; Mimoun, David] Univ Toulouse, SUPAERO, ISAE, F-31055 Toulouse, France.
[Lognonne, Philippe; Kawamura, Taichi] Univ Paris, Inst Phys Globe Paris, F-75205 Paris 13, France.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Ralph.Lorenz@jhuapl.edu
RI Lorenz, Ralph/B-8759-2016; Lognonne, Philippe/F-8846-2010; MIMOUN,
DAVID/M-7074-2016
OI Lorenz, Ralph/0000-0001-8528-4644; MIMOUN, DAVID/0000-0002-3427-2974
FU National Aeronautics and Space Administration (NASA) Mars Fundamental
Research and Mars Data Analysis programs [NNX12AJ47G, NNX12AI04G]
FX R. L. acknowledges the support of the National Aeronautics and Space
Administration (NASA) Mars Fundamental Research and Mars Data Analysis
programs, via Grants NNX12AJ47G and NNX12AI04G. The results reported
here benefited from the contributions of many individuals at the Jet
Propulsion Laboratory, Institut de Physique du Globe, Goldstone,
University of California- Los Angeles, and California Institute of
Technology (Caltech): we particularly acknowledge Paul Davis and Rob
Clayton for loan of equipment and determination of the seismic
properties of the playa. We thank Jim Murphy and an anonymous reviewer
for constructive comments. Special thanks to Dennis Mullen and Marie
Massey and the staff of the Goldstone Deep Space Network facility for
invaluable planning and logistical support.
NR 29
TC 2
Z9 2
U1 2
U2 12
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0037-1106
EI 1943-3573
J9 B SEISMOL SOC AM
JI Bull. Seismol. Soc. Amer.
PD DEC
PY 2015
VL 105
IS 6
BP 3015
EP 3023
DI 10.1785/0120150133
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CX7PX
UT WOS:000365895600014
ER
PT J
AU Knuth, KH
Habeck, M
Malakar, NK
Mubeen, AM
Placek, B
AF Knuth, Kevin H.
Habeck, Michael
Malakar, Nabin K.
Mubeen, Asim M.
Placek, Ben
TI Bayesian evidence and model selection
SO DIGITAL SIGNAL PROCESSING
LA English
DT Article
DE Bayesian signal processing; Bayesian evidence; Model testing; Nested
sampling; Odds ratio
ID LATENT GAUSSIAN MODELS; MONTE-CARLO METHODS; AUTOREGRESSIVE MODELS;
EVIDENCE FRAMEWORK; VARIATIONAL BAYES; NEURAL-NETWORKS; DARK ENERGY;
INFERENCE; CLASSIFICATION; EFFICIENT
AB In this paper we review the concepts of Bayesian evidence and Bayes factors, also known as log odds ratios, and their application to model selection. The theory is presented along with a discussion of analytic, approximate and numerical techniques. Specific attention is paid to the Laplace approximation, variational Bayes, importance sampling, thermodynamic integration, and nested sampling and its recent variants. Analogies to statistical physics, from which many of these techniques originate, are discussed in order to provide readers with deeper insights that may lead to new techniques. The utility of Bayesian model testing in the domain sciences is demonstrated by presenting four specific practical examples considered within the context of signal processing in the areas of signal detection, sensor characterization, scientific model selection and molecular force characterization. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Knuth, Kevin H.; Mubeen, Asim M.; Placek, Ben] SUNY Albany, Dept Phys, Albany, NY 12222 USA.
[Knuth, Kevin H.] SUNY Albany, Dept Informat, Albany, NY 12222 USA.
[Habeck, Michael] Max Planck Inst Biophys Chem, D-37077 Gottingen, Germany.
[Habeck, Michael] Univ Gottingen, Felix Bernstein Inst Math Stat Biosci, D-37077 Gottingen, Germany.
[Malakar, Nabin K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mubeen, Asim M.] Nathan S Kline Inst Psychiat Res, Div Geriatr, Orangeburg, NY 10962 USA.
RP Knuth, KH (reprint author), SUNY Albany, Dept Phys, Albany, NY 12222 USA.
EM kknuth@albany.edu
OI Malakar, Nabin/0000-0002-4816-6304
FU University at Albany; Deutsche Forschungsgemeinschaft (DFG) [HA
5918/1-1]; Jet Propulsion Laboratory, California Institute of
Technology; National Aeronautics and Space Administration
FX This paper was written for a special issue dedicated to William J.
Fitzgerald. While only once did I (Knuth) have the pleasure to meet
Prof. Fitzgerald, I was influenced by him indirectly through several of
his students, Ali Taylan Cemgil, Ercan E. Kuruoglu, and Robin D. Morris,
who in addition to always speaking very highly of him were each clearly
excellently trained as creative, talented and responsible members of the
scientific community. This research was supported in part by a
University at Albany Faculty Research Awards Program (FRAP-A) Award
(Knuth), a Deutsche Forschungsgemeinschaft (DFG) grant HA 5918/1-1
(Habeck) as well as two University at Albany Benevolent Research Grant
Awards (Malakar and Mubeen). Additional N. Malakar support carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
The authors would like to thank the anonymous reviewers for their
careful, thorough, and extensive comments, which have served to improve
the quality of this manuscript.
NR 134
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Z9 4
U1 1
U2 13
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1051-2004
EI 1095-4333
J9 DIGIT SIGNAL PROCESS
JI Digit. Signal Prog.
PD DEC
PY 2015
VL 47
BP 50
EP 67
DI 10.1016/j.dsp.2015.06.012
PG 18
WC Engineering, Electrical & Electronic
SC Engineering
GA CY0BU
UT WOS:000366072000007
ER
PT J
AU Bieniek, PA
Bhatt, US
Walker, DA
Raynolds, MK
Comiso, JC
Epstein, HE
Pinzon, JE
Tucker, CJ
Thoman, RL
Tran, H
Molders, N
Steele, M
Zhang, JL
Ermold, W
AF Bieniek, Peter A.
Bhatt, Uma S.
Walker, Donald A.
Raynolds, Martha K.
Comiso, Josefino C.
Epstein, Howard E.
Pinzon, Jorge E.
Tucker, Compton J.
Thoman, Richard L.
Huy Tran
Moelders, Nicole
Steele, Michael
Zhang, Jinlun
Ermold, Wendy
TI Climate Drivers Linked to Changing Seasonality of Alaska Coastal Tundra
Vegetation Productivity
SO EARTH INTERACTIONS
LA English
DT Article
DE Geographic location/entity; Arctic; Land surface; Atmosphere-ocean
structure/phenomena; Vegetation; Physical Meteorology and Climatology;
Climate variability
ID ARCTIC SEA-ICE; NORTHERN ALASKA; AIR-TEMPERATURE; TIME-SERIES; TRENDS;
WINTER; FIELD; TELECONNECTIONS; PRECIPITATION; AMPLIFICATION
AB The mechanisms driving trends and variability of the normalized difference vegetation index (NDVI) for tundra in Alaska along the Beaufort, east Chukchi, and east Bering Seas for 1982-2013 are evaluated in the context of remote sensing, reanalysis, and meteorological station data as well as regional modeling. Over the entire season the tundra vegetation continues to green; however, biweekly NDVI has declined during the early part of the growing season in all of the Alaskan tundra domains. These springtime declines coincide with increased snow depth in spring documented in northern Alaska. The tundra region generally has warmed over the summer but intraseasonal analysis shows a decline in midsummer land surface temperatures. The midsummer cooling is consistent with recent large-scale circulation changes characterized by lower sea level pressures, which favor increased cloud cover. In northern Alaska, the sea-breeze circulation is strengthened with an increase in atmospheric moisture/cloudiness inland when the land surface is warmed in a regional model, suggesting the potential for increased vegetation to feedback onto the atmospheric circulation that could reduce midsummer temperatures. This study shows that both large-and local-scale climate drivers likely play a role in the observed seasonality of NDVI trends.
C1 [Bieniek, Peter A.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Bieniek, Peter A.] Univ Alaska Fairbanks, Dept Atmospher Sci, Fairbanks, AK USA.
[Bieniek, Peter A.] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK USA.
[Walker, Donald A.; Raynolds, Martha K.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA.
[Walker, Donald A.; Raynolds, Martha K.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK USA.
[Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Epstein, Howard E.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA.
[Pinzon, Jorge E.; Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Thoman, Richard L.] NOAA, Natl Weather Serv, Fairbanks, AK USA.
[Huy Tran] Utah State Univ, Bingham Entrepreneurship & Energy Res Ctr, Vernal, UT USA.
[Steele, Michael; Zhang, Jinlun; Ermold, Wendy] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
RP Bieniek, PA (reprint author), 930 Koyukuk Dr,POB 757340, Fairbanks, AK 99775 USA.
EM pbieniek@alaska.edu
FU NSF Grants [ARC-051180, ARC-0902175, ARC-0902042, ARC-0901987]; NASA
[NNG6NEA00A, NNX13AE29G]; USGS Alaska Climate Science Center; University
of Alaska Fairbanks Office of the Vice Chancellor for Research
FX The authors thank Jim Overland, John Walsh, Matthew Sturm, Torre
Jorgenson, Xiangdong Zhang, Debasish Pai Mazumder, Ann Fienup-Riordan,
Alice Reardon, Mark John, the members of the Calista Elders Council, and
the two anonymous reviewers for their fruitful discussions that helped
to improve this study. This study was supported by funds from NSF Grants
ARC-051180, ARC-0902175, ARC-0902042, and ARC-0901987, NASA Grants
NNG6NEA00A and NNX13AE29G, the USGS Alaska Climate Science Center, and
the University of Alaska Fairbanks Office of the Vice Chancellor for
Research.
NR 84
TC 4
Z9 4
U1 8
U2 46
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1087-3562
J9 EARTH INTERACT
JI Earth Interact.
PD DEC
PY 2015
VL 19
AR 19
DI 10.1175/EI-D-15-0013.1
PG 29
WC Geosciences, Multidisciplinary
SC Geology
GA CY4OZ
UT WOS:000366389100001
ER
PT J
AU Dilmanian, FA
Eley, JG
Rusek, A
Krishnan, S
AF Dilmanian, F. Avraham
Eley, John G.
Rusek, Adam
Krishnan, Sunil
TI Charged Particle Therapy with Mini-Segmented Beams
SO FRONTIERS IN ONCOLOGY
LA English
DT Article
DE proton therapy; light-ion therapy; carbon therapy; proton minibeams;
light-ion minibeams; carbon minibeams; tissue-sparing effect;
interleaved carbon minibeams
ID X-RAY MICROBEAMS; MICROPLANAR BEAMS; MOUSE-BRAIN; RADIATION-THERAPY;
SPINAL-CORD; RADIOSURGERY; TISSUE; TUMORS; IRRADIATION; TOLERANCE
AB One of the fundamental attributes of proton therapy and carbon ion therapy is the ability of these charged particles to spare tissue distal to the targeted tumor. This significantly reduces normal tissue toxicity and has the potential to translate to a wider therapeutic index. Although, in general, particle therapy also reduces dose to the proximal tissues, particularly in the vicinity of the target, dose to the skin and to other very superficial tissues tends to be higher than that of megavoltage x-rays. The methods presented here, namely, "interleaved carbon minibeams" and "radiosurgery with arrays of proton and light ion minibeams," both utilize beams segmented into arrays of parallel "minibeams" of about 0.3 mm incident-beam size. These minibeam arrays spare tissues, as demonstrated by synchrotron x-ray experiments. An additional feature of particle minibeams is their gradual broadening due to multiple Coulomb scattering as they penetrate tissues. In the case of interleaved carbon minibeams, which do not broaden much, two arrays of planar carbon minibeams that remain parallel at target depth, are aimed at the target from 90 angles and made to "interleave" at the target to produce a solid radiation field within the target. As a result, the surrounding tissues are exposed only to individual carbon minibeam arrays and are therefore spared. The method was used in four-directional geometry at the NASA Space Radiation Laboratory to ablate a 6.5-mm target in a rabbit brain at a single exposure with 40 Gy physical absorbed dose. Contrast enhanced magnetic resonance imaging and histology 6-month later showed very focal target necrosis with nearly no damage to the surrounding brain. As for minibeams of protons and light ions, for which the minibeam broadening is substantial, measurements at MD Anderson Cancer Center in Houston, TX, USA; and Monte Carlo simulations showed that the broadening minibeams will merge with their neighbors at a certain tissue depth to produce a solid beam to treat the target. The resulting sparing of proximal normal tissue allows radiosurgical ablative treatments with smaller impact on the skin and shallow tissues. This report describes these two methods and discusses their potential clinical applications.
C1 [Dilmanian, F. Avraham] SUNY Stony Brook, Dept Radiat Oncol, Hlth Sci Ctr, Stony Brook, NY 11794 USA.
[Dilmanian, F. Avraham] SUNY Stony Brook, Dept Neurol, Hlth Sci Ctr, Stony Brook, NY 11794 USA.
[Dilmanian, F. Avraham] SUNY Stony Brook, Dept Radiol, Hlth Sci Ctr, Stony Brook, NY 11794 USA.
[Eley, John G.] Univ Maryland, Sch Med, Dept Radiat Oncol, Baltimore, MD 21201 USA.
[Rusek, Adam] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Rusek, Adam] NASA, Space Radiat Lab, Upton, NY USA.
[Krishnan, Sunil] Univ Texas MD Anderson Canc Ctr, Dept Radiat Oncol, Houston, TX 77030 USA.
RP Dilmanian, FA (reprint author), SUNY Stony Brook, Dept Radiat Oncol, Hlth Sci Ctr, Stony Brook, NY 11794 USA.
EM avraham.dilmanian@stonybrook.edu
FU Musella Brain Tumor Foundation; Voices against Brain Cancer; Concerned
Women of the Grove; Stony Brook's Targeted Research Opportunities
Program; Radiation Oncology Departments of Stony Brook University; MD
Anderson Cancer Center; Stony Brook Cancer Center, Radiation Oncology,
and Radiology
FX The studies presented in this report were supported by grants from the
Musella Brain Tumor Foundation, Voices against Brain Cancer, Concerned
Women of the Grove, and the Stony Brook's Targeted Research
Opportunities Program. Supports were also provided by the Radiation
Oncology Departments of Stony Brook University and MD Anderson Cancer
Center. One of us (ED) thanks Stony Brook Cancer Center, Radiation
Oncology, and Radiology for support, and one of us (SK) acknowledges the
John E. and Dorothy J. Harris Endowment Professorship. We also thank
Tiffany Bowman and Katherine Gebhart for assistance with graphic arts.
NR 25
TC 0
Z9 0
U1 1
U2 3
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 2234-943X
J9 FRONT ONCOL
JI Front. Oncol.
PD DEC 1
PY 2015
VL 5
AR 269
DI 10.3389/fonc.2015.00269
PG 8
WC Oncology
SC Oncology
GA CY3UO
UT WOS:000366335600002
PM 26649281
ER
PT J
AU Ruzmaikin, A
Aumann, HH
Jiang, JH
AF Ruzmaikin, Alexander
Aumann, Hartmut H.
Jiang, Jonathan H.
TI Interhemispheric Variability of Earth's Radiation
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Atm; Ocean Structure; Phenomena; Atmosphere-ocean interaction;
Observational techniques and algorithms; Climate records; Satellite
observations; Variability; Climate variability; Interannual variability;
Oceanic variability
ID INTERTROPICAL CONVERGENCE ZONE; GLOBAL CLIMATE MODEL; ATMOSPHERE
RADIATION; OCEAN; SLOWDOWN; BIASES; CMIP5
AB The variability of interhemispheric symmetry of Earth's energy serves as an independent indicator of climate change. The analysis of updated data obtained from satellite measurements at the top of the atmosphere (TOA) shows that in accord with Earth's orbital requirements the annually averaged incident solar radiation is the same in the Northern and Southern Hemispheres, the annual mean of the reflected shortwave radiation is almost north-south symmetric, and the annual mean of the outgoing longwave radiation is larger in the Northern Hemisphere by 1.4 W m(-2). These mean radiations systematically differ from the mean radiations found from the numerical atmospheric models that participated in the Coupled Model Intercomparison Project phase 5 (CMIP5). The hemispheric differences of the TOA radiations vary on the annual and interannual time scales. The multidecadal variability in Earth's north-south temperature difference reveals a similarity of trends in both hemispheres. The Atlantic meridional transport (in contrast to the Pacific meridional transport) is found to be coherent with the interhemispheric ocean heat content (OHC) difference on decadal and multidecadal time scales, indicating a critical role of the Atlantic in the interhemispheric energy balance change.
C1 [Ruzmaikin, Alexander; Aumann, Hartmut H.; Jiang, Jonathan H.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ruzmaikin, A (reprint author), Jet Prop Lab, Mail Stop 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alexander.ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology;
National Aeronautics and Space Administration
FX We thank David Doelling for the help with understanding the CERES data.
We are grateful to the reviewers for helpful comments. This work was
supported in part by the Jet Propulsion Laboratory of the California
Institute of Technology under a contract with the National Aeronautics
and Space Administration.
NR 45
TC 1
Z9 1
U1 4
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD DEC
PY 2015
VL 72
IS 12
BP 4615
EP 4628
DI 10.1175/JAS-D-15-0106.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CY3TP
UT WOS:000366333100001
ER
PT J
AU Atli, KC
Karaman, I
Noebe, RD
Bigelow, G
Gaydosh, D
AF Atli, K. C.
Karaman, I.
Noebe, R. D.
Bigelow, G.
Gaydosh, D.
TI Work production using the two-way shape memory effect in NiTi and a
Ni-rich NiTiHf high-temperature shape memory alloy
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE high temperature shape memory alloys; martensitic transformation;
two-way shape memory effect; work output; thermomechanical training
ID ZN-AL ALLOYS; MARTENSITIC-TRANSFORMATION; DEFORMATION; MICROSTRUCTURE;
PHASE; BEHAVIOR; STRESS
AB The work output capacity of the two-way shape memory effect (TWSME) in a Ni50.3Ti29.7Hf20 (at%) high-temperature shape memory alloy (HTSMA) was investigated and compared to that of binary Ni49.9Ti50.1 (at%). TWSME was induced through a training procedure of 100 thermomechanical cycles under different tensile stresses. It was observed that TWSME in as-extruded and trained Ni50.3Ti29.7Hf20 could produce 0.7% strain against a compressive stress of 100 MPa, corresponding to a maximum work output of 0.08 J g(-1), compared to a maximum value of 0.06 J g(-1) for binary NiTi. A peak aging heat treatment of 3 h at 550 degrees C, which previously has been shown to result in near-perfect functional stability in Ni50.3Ti29.7Hf20 during isobaric thermal cycling, did not improve the TWSME and actually resulted in a decrease in the magnitude and stability of the TWSME and its work output capacity. Nevertheless, the magnitude of TWSM behavior of Ni50.3Ti29.7Hf20, in the absence of an aging heat treatment, renders it an attractive candidate for high-temperature TWSM actuation.
C1 [Atli, K. C.] Anadolu Univ, Dept Mech Engn, Eskisehir, Turkey.
[Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
[Noebe, R. D.; Bigelow, G.; Gaydosh, D.] NASA Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Gaydosh, D.] Ohio Aerosp Inst, Cleveland, OH USA.
RP Atli, KC (reprint author), Anadolu Univ, Dept Mech Engn, Eskisehir, Turkey.
EM kcatli@anadolu.edu.tr
RI Atli, Kadri/D-6978-2013
OI Atli, Kadri/0000-0002-4807-2113
FU NASA Fundamental Aeronautics Program, Subsonic Fixed Wing project
[NNX07AB56A]; FAP Aeronautical Sciences Project; TAC Transformational
Tools & Technologies Project, Discipline Lead, Dale Hopkins; US Air
Force Office of Scientific Research [FA9550-15-0287]
FX This study was originally supported by the NASA Fundamental Aeronautics
Program, Subsonic Fixed Wing project through Cooperative Agreement no.
NNX07AB56A, with additional support from the FAP Aeronautical Sciences
Project and the TAC Transformational Tools & Technologies Project,
Discipline Lead, Dale Hopkins. The work performed at Texas A&M
University was supported by the US Air Force Office of Scientific
Research, under grant no. FA9550-15-0287. The authors wish to thank the
Shape Memory Alloy Group at NASA Glenn Research Center for helpful
discussions.
NR 41
TC 0
Z9 0
U1 8
U2 21
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD DEC
PY 2015
VL 24
IS 12
AR 125023
DI 10.1088/0964-1726/24/12/125023
PG 12
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA CY0QV
UT WOS:000366111500024
ER
PT J
AU Milligan, RO
AF Milligan, Ryan O.
TI Extreme Ultra-Violet Spectroscopy of the Lower Solar Atmosphere During
Solar Flares
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT Conference on Solar and Stellar Flares - Observations, Simulations and
Synergies
CY JUN 23-27, 2014
CL Prague, CZECH REPUBLIC
DE Chromosphere, active; Flares, dynamics; Flares, impulsive phase; Flares,
spectrum; Heating, chromospheric; Heating, in flares; Spectral line,
broadening; Spectral line, intensity and diagnostics; Spectrum,
continuum; Spectrum, ultraviolet
ID ULTRAVIOLET IMAGING SPECTROMETER; WHITE-LIGHT FLARES; HARD X-RAY; HIGH
TIME RESOLUTION; GENTLE CHROMOSPHERIC EVAPORATION; DIFFERENTIAL EMISSION
MEASURES; GENERAL SPECTRAL PROPERTIES; IMPULSIVE PHASE; ACTIVE-REGION;
LYMAN-CONTINUUM
AB The extreme ultra-violet (EUV) portion of the solar spectrum contains a wealth of diagnostic tools for probing the lower solar atmosphere in response to an injection of energy, particularly during the impulsive phase of solar flares. These include temperature- and density-sensitive line ratios, Doppler-shifted emission lines, nonthermal broadening, abundance measurements, differential emission measure profiles, continuum temperatures and energetics, among others. In this article I review some of the recent advances that have been made using these techniques to infer physical properties of heated plasma at footpoint and ribbon locations during the initial stages of solar flares. I primarily focus on studies that have utilised spectroscopic EUV data from Hinode/EUV Imaging Spectrometer (EIS) and Solar Dynamics Observatory/EUV Variability Experiment (SDO/EVE), and I also provide some historical background and a summary of future spectroscopic instrumentation.
C1 [Milligan, Ryan O.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Milligan, Ryan O.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Div, Greenbelt, MD 20771 USA.
[Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Milligan, RO (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
EM r.milligan@qub.ac.uk
FU NASA for LWS/TRT grant [NNX11AQ53G]; LWS/SDO Data Analysis grant
[NNX14AE07G]
FX The author is grateful for financial support from NASA for LWS/TR&T
grant NNX11AQ53G and LWS/SDO Data Analysis grant NNX14AE07G. He also
thanks Brian Dennis, Mihalis Mathioudakis, Peter Young, Hugh Hudson,
Helen Mason, David Graham, Lyndsay Fletcher (Guest Editor) and the
anonymous referee for their useful comments and feedback on the
manuscript, as well as the organisers of the meeting on Solar and
Stellar Flares: Observations, Simulations, and Synergies in Prague,
Czech Republic in June 2014 for the invitation to present this review.
NR 142
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U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2015
VL 290
IS 12
BP 3399
EP 3423
DI 10.1007/s11207-015-0748-2
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY0ZP
UT WOS:000366136000003
ER
PT J
AU Kowalski, AF
Hawley, SL
Carlsson, M
Allred, JC
Uitenbroek, H
Osten, RA
Holman, G
AF Kowalski, Adam F.
Hawley, S. L.
Carlsson, M.
Allred, J. C.
Uitenbroek, H.
Osten, R. A.
Holman, G.
TI New Insights into White-Light Flare Emission from Radiative-Hydrodynamic
Modeling of a Chromospheric Condensation
SO SOLAR PHYSICS
LA English
DT Article; Proceedings Paper
CT Conference on Solar and Stellar Flares - Observations, Simulations and
Synergies
CY JUN 23-27, 2014
CL Prague, CZECH REPUBLIC
DE Flares, dynamics; Flares, energetic particles; Flares, impulsive phase;
Flares, models; Flares, spectrum; Flares, white-light
ID STAR YZ CMI; IMPULSIVE SOLAR-FLARES; EQUATION-OF-STATE; X-RAY-EMISSION;
HYDROGEN LINES; MULTIWAVELENGTH OBSERVATIONS; OPTICAL-SPECTRA; STELLAR
FLARES; AD LEONIS; NONTHERMAL ELECTRONS
AB The heating mechanism at high densities during M-dwarf flares is poorly understood. Spectra of M-dwarf flares in the optical and near-ultraviolet wavelength regimes have revealed three continuum components during the impulsive phase: 1) an energetically dominant blackbody component with a color temperature of in the blue-optical, 2) a smaller amount of Balmer continuum emission in the near-ultraviolet at , and 3) an apparent pseudo-continuum of blended high-order Balmer lines between and . These properties are not reproduced by models that employ a typical "solar-type" flare heating level of in nonthermal electrons, and therefore our understanding of these spectra is limited to a phenomenological three-component interpretation. We present a new 1D radiative-hydrodynamic model of an M-dwarf flare from precipitating nonthermal electrons with a high energy flux of . The simulation produces bright near-ultraviolet and optical continuum emission from a dense (), hot () chromospheric condensation. For the first time, the observed color temperature and Balmer jump ratio are produced self-consistently in a radiative-hydrodynamic flare model. We find that a blackbody-like continuum component and a low Balmer jump ratio result from optically thick Balmer () and Paschen recombination () radiation, and thus the properties of the flux spectrum are caused by blue ( ) light escaping over a larger physical depth range than by red ( ) and near-ultraviolet ( ) light. To model the near-ultraviolet pseudo-continuum previously attributed to overlapping Balmer lines, we include the extra Balmer continuum opacity from Landau-Zener transitions that result from merged, high-order energy levels of hydrogen in a dense, partially ionized atmosphere. This reveals a new diagnostic of ambient charge density in the densest regions of the atmosphere that are heated during dMe and solar flares.
C1 [Kowalski, Adam F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kowalski, Adam F.; Allred, J. C.; Holman, G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Hawley, S. L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Carlsson, M.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Uitenbroek, H.] Natl Solar Observ, Sunspot, NM 88349 USA.
[Osten, R. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Kowalski, AF (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM adam.f.kowalski@nasa.gov
FU NASA; University of Maryland Goddard Planetary Heliophysics Institute
(GPHI) [132]
FX Adam F. Kowalski thanks the Science Organizing Committee of the Solar
and Stellar Flares meeting in Prague, Czech Republic for the opportunity
to present this work. We thank an anonymous referee for clarifications
and comments that helped improve this work. Adam F. Kowalski thanks Petr
Heinzel and Hans Ludwig for bringing hot star modeling articles of Stark
broadening to his attention. We thank Adrian Daw, Eric Agol, Ellen
Zweibel, and Jeremiah Murphy for helpful discussions and William Abbett
for several IDL routines used in the analysis. AFK also acknowledges
helpful discussions at the International Space Science Institute with
Lyndsay Fletcher's Solar and Stellar Flares team and with Sven
Wedemeyer-Bohm's Magnetic Activity of M-type Dwarf Stars and the
Influence on Habitable Extra-solar Planets team. This research was
supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA, and by the University of
Maryland Goddard Planetary Heliophysics Institute (GPHI) Task 132.
NR 119
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U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD DEC
PY 2015
VL 290
IS 12
BP 3487
EP 3523
DI 10.1007/s11207-015-0708-x
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY0ZP
UT WOS:000366136000006
ER
PT J
AU Cochran, AL
Levasseur-Regourd, AC
Cordiner, M
Hadamcik, E
Lasue, J
Gicquel, A
Schleicher, DG
Charnley, SB
Mumma, MJ
Paganini, L
Bockelee-Morvan, D
Biver, N
Kuan, YJ
AF Cochran, Anita L.
Levasseur-Regourd, Anny-Chantal
Cordiner, Martin
Hadamcik, Edith
Lasue, Jeremie
Gicquel, Adeline
Schleicher, David G.
Charnley, Steven B.
Mumma, Michael J.
Paganini, Lucas
Bockelee-Morvan, Dominique
Biver, Nicolas
Kuan, Yi-Jehng
TI The Composition of Comets
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Comets; Origins; Taxonomy; Rosetta
ID O1 HALE-BOPP; NARROW-BAND PHOTOMETRY; FORBIDDEN OXYGEN LINES;
JUPITER-FAMILY COMETS; INTERPLANETARY DUST PARTICLES; INFRARED SPECTRAL
SURVEY; C/2004 Q2 MACHHOLZ; DEEP-IMPACT EVENT; IKEYA-SEKI 1965F;
ORTHO-PARA RATIO
AB This paper is the result of the International Cometary Workshop, held in Toulouse, France in April 2014, where the participants came together to assess our knowledge of comets prior to the ESA Rosetta Mission. In this paper, we look at the composition of the gas and dust from the comae of comets. With the gas, we cover the various taxonomic studies that have broken comets into groups and compare what is seen at all wavelengths. We also discuss what has been learned from mass spectrometers during flybys. A few caveats for our interpretation are discussed. With dust, much of our information comes from flybys. They include in situ analyses as well as samples returned to Earth for laboratory measurements. Remote sensing IR observations and polarimetry are also discussed. For both gas and dust, we discuss what instruments the Rosetta spacecraft and Philae lander will bring to bear to improve our understanding of comet 67P/Churyumov-Gerasimenko as "ground-truth" for our previous comprehensive studies. Finally, we summarize some of the initial Rosetta Mission findings.
C1 [Cochran, Anita L.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Levasseur-Regourd, Anny-Chantal] UPMC, LATMOS, Paris, France.
[Cordiner, Martin; Gicquel, Adeline; Charnley, Steven B.; Mumma, Michael J.; Paganini, Lucas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hadamcik, Edith] UPMC, LATMOS, Guyancourt, France.
[Lasue, Jeremie] UPS, IRAP, Toulouse, France.
[Gicquel, Adeline] MPS, Gottingen, Germany.
[Schleicher, David G.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Bockelee-Morvan, Dominique; Biver, Nicolas] Observ Paris, LESIA, Meudon, France.
[Kuan, Yi-Jehng] Natl Taiwan Normal Univ, Taipei, Taiwan.
RP Cochran, AL (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
EM anita@astro.as.utexas.edu
FU CNES (the French Space Agency)
FX The authors would like to thank Dr. Paul Feldman, Dr. Jacques Crovisier,
Dr. Neil Dello Russo and Dr. Adam McKay for helpful comments and making
data available for our use. Partial support from CNES (the French Space
Agency) is acknowledged.
NR 210
TC 9
Z9 9
U1 2
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 197
IS 1-4
BP 9
EP 46
DI 10.1007/s11214-015-0183-6
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY4KN
UT WOS:000366377100002
ER
PT J
AU Bockelee-Morvan, D
Calmonte, U
Charnley, S
Duprat, J
Engrand, C
Gicquel, A
Hassig, M
Jehin, E
Kawakita, H
Marty, B
Milam, S
Morse, A
Rousselot, P
Sheridan, S
Wirstrom, E
AF Bockelee-Morvan, Dominique
Calmonte, Ursina
Charnley, Steven
Duprat, Jean
Engrand, Cecile
Gicquel, Adeline
Haessig, Myrtha
Jehin, Emmanuel
Kawakita, Hideyo
Marty, Bernard
Milam, Stefanie
Morse, Andrew
Rousselot, Philippe
Sheridan, Simon
Wirstrom, Eva
TI Cometary Isotopic Measurements
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Comets; Isotopes
ID INTERPLANETARY DUST PARTICLES; O1 HALE-BOPP; ULTRACARBONACEOUS ANTARCTIC
MICROMETEORITES; DENSE INTERSTELLAR CLOUDS; GRAIN SURFACE-CHEMISTRY;
SOLAR-SYSTEM; ABUNDANCE RATIO; DARK CLOUDS; C/1995 O1; LOW-MASS
AB Isotopic ratios in comets provide keys for the understanding of the origin of cometary material, and the physical and chemical conditions in the early Solar Nebula. We review here measurements acquired on the D/H, N-14/N-15, O-16/O-18, C-12/C-13, and S-32/S-34 ratios in cometary grains and gases, and discuss their cosmogonic implications. The review includes analyses of potential cometary material available in collections on Earth, recent measurements achieved with the Herschel Space Observatory, large optical telescopes, and Rosetta, as well as recent results obtained from models of chemical-dynamical deuterium fractionation in the early solar nebula. Prospects for future measurements are presented.
C1 [Bockelee-Morvan, Dominique] Univ Paris Diderot, UPMC, CNRS, Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Calmonte, Ursina] Univ Bern, Inst Phys, Space Res & Planetary Sci, CH-3012 Bern, Switzerland.
[Charnley, Steven; Milam, Stefanie] NASA, Goddard Space Flight Ctr Greenbelt, Astrochem Lab, Greenbelt, MD 20771 USA.
[Duprat, Jean; Engrand, Cecile] Univ Paris 11, CNRS, IN2P3, CSNSM,UMR 8609, F-91405 Orsay, France.
[Gicquel, Adeline] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Haessig, Myrtha] SW Res Inst, San Antonio, TX USA.
[Jehin, Emmanuel] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
[Kawakita, Hideyo] Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto 6038555, Japan.
[Marty, Bernard] Univ Lorraine, CNRS, CRPG, F-54500 Vandoeuvre Les Nancy, France.
[Morse, Andrew; Sheridan, Simon] Open Univ, Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Rousselot, Philippe] Univ Franche Comte, Inst UTINAM, Observ Sci Univers THETA, UMR CNRS 6213, F-25010 Besancon, France.
[Wirstrom, Eva] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden.
RP Bockelee-Morvan, D (reprint author), Univ Paris Diderot, UPMC, CNRS, Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM dominique.bockelee@obspm.fr
RI Milam, Stefanie/D-1092-2012;
OI Milam, Stefanie/0000-0001-7694-4129; Wirstrom, Eva/0000-0002-0656-876X
FU NASA; Swedish Space Board
FX This work was supported by NASA's Planetary Astronomy and Planetary
Atmospheres Programs (SNM and SBC), and by the Swedish Space Board
(ESW).
NR 219
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U1 6
U2 20
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 197
IS 1-4
BP 47
EP 83
DI 10.1007/s11214-015-0156-9
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY4KN
UT WOS:000366377100003
ER
PT J
AU Gudipati, MS
Abou Mrad, N
Blum, J
Charnley, SB
Chiavassa, T
Cordiner, MA
Mousis, O
Danger, G
Duvernay, F
Gundlach, B
Hartogh, P
Marboeuf, U
Simonia, I
Simonia, T
Theule, P
Yang, R
AF Gudipati, Murthy S.
Abou Mrad, Ninette
Blum, Juergen
Charnley, Steven B.
Chiavassa, Thierry
Cordiner, Martin A.
Mousis, Olivier
Danger, Gregoire
Duvernay, Fabrice
Gundlach, Bastian
Hartogh, Paul
Marboeuf, Ulysse
Simonia, Irakli
Simonia, Tsitsino
Theule, Patrice
Yang, Rui
TI Laboratory Studies Towards Understanding Comets
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Comets; Laboratory; Experimental; Ice; Volatiles; Clathrates; Origin of
life; Organics; Review; Isotope ratios; Negative ions; Coma; Outgassing;
Origin of solar systems
ID INTERSTELLAR ICE ANALOGS; OUTER SOLAR-SYSTEM; IN-SITU ANALYSIS;
PLANETARY-SCIENCE EXPERIMENTS; POLYCYCLIC AROMATIC MOLECULE; IONIZATION
MASS-SPECTROMETRY; CLATHRATE-HYDRATE FORMATION; CIRCULARLY-POLARIZED
LIGHT; ELECTRON-ATTACHMENT RATES; 2-STEP LASER-ABLATION
AB This review presents some of the recent advancements in our understanding of comets facilitated by laboratory studies, need for new laboratory simulations, and predictions for future explorations. With the spacecraft Rosetta at the comet 67P/Churyumov-Gerasimenko, a large volume of science data is expected to follow early results that have been published recently. The most surprising of them being hard ice shell that bounced the lander Philae a couple of times before settling on the comet. Long evaded molecular nitrogen has now been detected in the comet 67P/CG. The observed density of is in line with other comet observations, whereas the nature and composition of hydrocarbons detected on the surface are still a puzzle. Observation of D/H ratio that deviates significantly from Earth's water D/H ratio brings back to the table the long-standing question whether or not water on Earth was delivered by comet impacts. Our review summarizes some of the critical laboratory work that helps improve our understanding of cometary interior (whether amorphous or crystalline or containing clathrates), cometary surface (rich of complex organics), cometary coma and tail (D/H ratio, negative ions, and photoluminescence). Outstanding questions are also discussed.
C1 [Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Abou Mrad, Ninette; Chiavassa, Thierry; Danger, Gregoire; Duvernay, Fabrice; Theule, Patrice] Aix Marseille Univ, PIIM UMR CNRS 7345, F-13397 Marseille, France.
[Blum, Juergen; Gundlach, Bastian] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38196 Braunschweig, Germany.
[Charnley, Steven B.; Cordiner, Martin A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Mousis, Olivier] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Hartogh, Paul] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Marboeuf, Ulysse] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Marboeuf, Ulysse] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland.
[Simonia, Irakli; Simonia, Tsitsino] Ilia State Univ, Sch Nat Sci & Engn, Lab Interdisciplinary Invest Cosmochem & Astron, GE-0162 Tbilisi, Rep of Georgia.
[Yang, Rui] Univ Maryland, College Pk, MD 20742 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011
FU NASA; Spitzer Science Center; Astrobiology Institute Node Early
Habitable Environments (NASA Ames); JPL's DRDF; RTD; National
Aeronautics and Space Administration; A*MIDEX project - "Investissements
d'Avenir" French Government program [ANR-11-IDEX-0001-02]; French
national programs "Physique Chimie du Milieu Interstellaire" (P.C.M.I,
INSU); "Programme National de Planetologie" (P.N.P, INSU);
"Environnements Planetaires et Origines de la Vie" (E.P.O.V, CNRS);
"Centre National d'Etudes Spatiales" (C.N.E.S) from its exobiology
program; ANR project VAHIIA of the French Agence Nationale de la
Recherche [ANR-12-JS08-0001-01]; Swiss National Science Foundation;
Goddard Center for Astrobiology
FX Murthy Gudipati thanks partial funding from the following NASA programs:
Planetary Atmospheres, Cassini Data Analysis Programs, Spitzer Science
Center, and Astrobiology Institute Node Early Habitable Environments
(NASA Ames). JPL's DRDF and R&TD funding for infrastructure of the "ice
spectroscopy laboratory" is also gratefully acknowledged. This research
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. Olivier Mousis thanks the support of the A*MIDEX project
(no. ANR-11-IDEX-0001-02) funded by the "Investissements d'Avenir"
French Government program, managed by the French National Research
Agency (ANR). Gregoire Danger and collaborators thank funding by the
French national programs "Physique Chimie du Milieu Interstellaire"
(P.C.M.I, INSU), "Programme National de Planetologie" (P.N.P, INSU),
"Environnements Planetaires et Origines de la Vie" (E.P.O.V, CNRS) and
the "Centre National d'Etudes Spatiales" (C.N.E.S) from its exobiology
program as well as the ANR project VAHIIA (Grant ANR-12-JS08-0001-01) of
the French Agence Nationale de la Recherche. Ulysse Marboeuf thanks
funding from the Swiss National Science Foundation. The work of Steven
B. Charnley and Martin A. Cordiner was supported by NASA's Planetary
Atmospheres Program and the Goddard Center for Astrobiology.
NR 308
TC 1
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U1 10
U2 28
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 197
IS 1-4
BP 101
EP 150
DI 10.1007/s11214-015-0192-5
PG 50
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY4KN
UT WOS:000366377100005
ER
PT J
AU Willacy, K
Alexander, C
Ali-Dib, M
Ceccarelli, C
Charnley, SB
Doronin, M
Ellinger, Y
Gast, P
Gibb, E
Milam, SN
Mousis, O
Pauzat, F
Tornow, C
Wirstrom, ES
Zicler, E
AF Willacy, K.
Alexander, C.
Ali-Dib, M.
Ceccarelli, C.
Charnley, S. B.
Doronin, M.
Ellinger, Y.
Gast, P.
Gibb, E.
Milam, S. N.
Mousis, O.
Pauzat, F.
Tornow, C.
Wirstrom, E. S.
Zicler, E.
TI The Composition of the Protosolar Disk and the Formation Conditions for
Comets
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Protostellar disks; Solar nebula; Comets; Chemistry
ID EARLY SOLAR NEBULA; O1 HALE-BOPP; EVOLUTIONARY TURBULENT MODEL;
NUCLEAR-SPIN TEMPERATURES; DENSE INTERSTELLAR CLOUDS; WEAKLY MAGNETIZED
DISKS; LOCAL SHEAR INSTABILITY; PLANET FORMATION REGION; SHORT-PERIOD
COMETS; CO SNOW LINE
AB Conditions in the protosolar nebula have left their mark in the composition of cometary volatiles, thought to be some of the most pristine material in the solar system. Cometary compositions represent the end point of processing that began in the parent molecular cloud core and continued through the collapse of that core to form the protosun and the solar nebula, and finally during the evolution of the solar nebula itself as the cometary bodies were accreting. Disentangling the effects of the various epochs on the final composition of a comet is complicated. But comets are not the only source of information about the solar nebula. Protostellar disks around young stars similar to the protosun provide a way of investigating the evolution of disks similar to the solar nebula while they are in the process of evolving to form their own solar systems. In this way we can learn about the physical and chemical conditions under which comets formed, and about the types of dynamical processing that shaped the solar system we see today.
This paper summarizes some recent contributions to our understanding of both cometary volatiles and the composition, structure and evolution of protostellar disks.
C1 [Willacy, K.; Alexander, C.] NASA, CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ali-Dib, M.] Univ Franche Comte, CNRS INSU, Inst UTINAM, UMR 6213, F-25010 Besancon, France.
[Ceccarelli, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Ceccarelli, C.] CNRS, IPAG, F-38000 Grenoble, France.
[Charnley, S. B.; Milam, S. N.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Doronin, M.; Ellinger, Y.; Pauzat, F.; Zicler, E.] Univ Paris 06, Sorbonne Univ, CNRS UMR, LCT, F-75252 Paris 05, France.
[Doronin, M.] Univ Paris 06, Sorbonne Univ, CNRS UMR, LERMA LPMAA, F-75252 Paris 05, France.
[Gast, P.; Tornow, C.] Inst Planetary Res DLR, D-12489 Berlin, Germany.
[Gibb, E.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
[Mousis, O.] Aix Marseille Univ, CNRS, LAM, UMR 736, F-13388 Marseille, France.
[Wirstrom, E. S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
RP Willacy, K (reprint author), NASA, CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM karen.willacy@jpl.nasa.gov
RI Milam, Stefanie/D-1092-2012;
OI Milam, Stefanie/0000-0001-7694-4129; Wirstrom, Eva/0000-0002-0656-876X
FU National Aeronautics and Space Administration; Goddard Center for
Astrobiology; NASA Origins of Solar Systems Program; NASA [NNX11AG44G];
NSF [AST-1211362]; CNES; A*MIDEX project - "Investissements d'Avenir"
French government program [ANR-11-1DEX-0001-02]; city of Beancon;
Swedish National Space Board
FX The work of K. Willacy and C. Alexander was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. S.B.
Charnley and S.N. Milam acknowledge the support of the Goddard Center
for Astrobiology. Support for K. Willacy, S.B. Charnley and S.N. Milam
was partially provided by the NASA Origins of Solar Systems Program. E.
Gibb was supported by the NASA Exobiology and Evolutionary Biology
(grant NNX11AG44G) and NSF Planetary Astronomy (grant AST-1211362)
programs. O. Mousis and C. Ceccarelli acknowledge support from CNES.
Support for O. Mousis was provided by the A*MIDEX project (no.
ANR-11-1DEX-0001-02) funded by the "Investissements d'Avenir" French
government program managed by the French National Research Agency (ANR).
M. Ali-Dib was supported by a grant from the city of Beancon. E. S.
Wirstrom was supported by the Swedish National Space Board.
NR 215
TC 7
Z9 7
U1 2
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 197
IS 1-4
BP 151
EP 190
DI 10.1007/s11214-015-0167-6
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY4KN
UT WOS:000366377100006
ER
PT J
AU Mandt, KE
Mousis, O
Marty, B
Cavalie, T
Harris, W
Hartogh, P
Willacy, K
AF Mandt, K. E.
Mousis, O.
Marty, B.
Cavalie, T.
Harris, W.
Hartogh, P.
Willacy, K.
TI Constraints from Comets on the Formation and Volatile Acquisition of the
Planets and Satellites
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar system formation; Comets; Atmospheres; Giant planets; Terrestrial
planets; Moon formation
ID PROBE MASS-SPECTROMETER; SHOEMAKER-LEVY 9; O1 HALE-BOPP; HELIUM
INTERFEROMETER EXPERIMENT; EVOLUTIONARY TURBULENT MODEL; HERSCHEL-PACS
OBSERVATIONS; NEPTUNES CARBON-MONOXIDE; ODIN SPACE TELESCOPE; ISO-SWS
OBSERVATIONS; EARLY SOLAR-SYSTEM
AB Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.
C1 [Mandt, K. E.] SW Res Inst, San Antonio, TX 78227 USA.
[Mousis, O.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Marty, B.] Nancy Univ, CRPG CNRS, Vandoeuvre Les Nancy, France.
[Cavalie, T.; Hartogh, P.] Max Planck Inst Solar Syst Res, Gottingen, Germany.
[Harris, W.] Univ Arizona, Tucson, AZ USA.
[Willacy, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mandt, KE (reprint author), SW Res Inst, San Antonio, TX 78227 USA.
EM kmandt@swri.edu
OI Mandt, Kathleen/0000-0001-8397-3315
FU JPL [1345493]; NASA [NNX13AQ99G]; CNES; A*MIDEX project -
"Investissements d'Avenir" French Government program
[ANR-11-IDEX-0001-02]; National Aeronautics and Space Administration;
NASA/Origins of Solar Systems program; European Research Council
[267255]
FX K.E.M. acknowledges support from JPL Subcontract 1345493 and NASA grant
NNX13AQ99G. O.M. acknowledges support from CNES. The work contributed by
O.M. was carried out thanks to the support of the A*MIDEX project (no.
ANR-11-IDEX-0001-02) funded by the "Investissements d'Avenir" French
Government program, managed by the French National Research Agency
(ANR). The work contributed by K.W. was carried out at the Jet
Propulsion Laboratory/California Institute of Technology, under contract
with the National Aeronautics and Space Administration with partial
support from the NASA/Origins of Solar Systems program. B.M.
acknowledges support from the European Research Council (grant agreement
number 267255).
NR 285
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U1 3
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 197
IS 1-4
BP 297
EP 342
DI 10.1007/s11214-015-0161-z
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CY4KN
UT WOS:000366377100009
ER
PT J
AU Pauwels, VRN
De Lannoy, GJM
AF Pauwels, Valentijn R. N.
De Lannoy, Gabrielle J. M.
TI Error covariance calculation for forecast bias estimation in hydrologic
data assimilation
SO ADVANCES IN WATER RESOURCES
LA English
DT Article
DE Data assimilation; Bias; Kalman filter
ID KALMAN FILTER; SYSTEM
AB To date, an outstanding issue in hydrologic data assimilation is a proper way of dealing with forecast bias. A frequently used method to bypass this problem is to rescale the observations to the model climatology. While this approach improves the variability in the modeled soil wetness and discharge, it is not designed to correct the results for any bias. Alternatively, attempts have been made towards incorporating dynamic bias estimates into the assimilation algorithm. Persistent bias models are most often used to propagate the bias estimate, where the a priori forecast bias error covariance is calculated as a constant fraction of the unbiased a priori state error covariance. The latter approach is a simplification to the explicit propagation of the bias error covariance. The objective of this paper is to examine to which extent the choice for the propagation of the bias estimate and its error covariance influence the filter performance. An Observation System Simulation Experiment (OSSE) has been performed, in which ground water storage observations are assimilated into a biased conceptual hydrologic model. The magnitudes of the forecast bias and state error covariances are calibrated by optimizing the innovation statistics of groundwater storage. The obtained bias propagation models are found to be identical to persistent bias models. After calibration, both approaches for the estimation of the forecast bias error covariance lead to similar results, with a realistic attribution of error variances to the bias and state estimate, and significant reductions of the bias in both the estimates of groundwater storage and discharge. Overall, the results in this paper justify the use of the traditional approach for online bias estimation with a persistent bias model and a simplified forecast bias error covariance estimation. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Pauwels, Valentijn R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia.
[Pauwels, Valentijn R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia.
[De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pauwels, VRN (reprint author), Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia.
EM Valentijn.Pauwels@monash.edu
OI Pauwels, Valentijn/0000-0002-1290-9313
FU Australian Research Council [FT130100545]
FX Valentijn Pauvvels is currently funded by the Australian Research
Council (grant no. FT130100545) through the Future Fellowship scheme. We
thank the Department Operational Water Management of the Flemish
Environmental Agency (Belgium) for providing the discharge and the
meteorological data.
NR 31
TC 2
Z9 2
U1 2
U2 7
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0309-1708
EI 1872-9657
J9 ADV WATER RESOUR
JI Adv. Water Resour.
PD DEC
PY 2015
VL 86
BP 284
EP 296
DI 10.1016/j.advwatres.2015.05.013
PN B
PG 13
WC Water Resources
SC Water Resources
GA CX3TY
UT WOS:000365623500004
ER
PT J
AU English, KL
Lee, SMC
Loehr, JA
Ploutz-Snyder, RJ
Ploutz-Snyder, LL
AF English, Kirk L.
Lee, Stuart M. C.
Loehr, James A.
Ploutz-Snyder, Robert J.
Ploutz-Snyder, Lori L.
TI Isokinetic Strength Changes Following Long-Duration Spaceflight on the
ISS
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE ARED; gender; disuse; iRED; ISS; microgravity; muscle
ID INTERNATIONAL-SPACE-STATION; SKELETAL-MUSCLE; RESISTANCE EXERCISE;
RESISTIVE EXERCISE; BED REST; HUMANS; WOMEN; MEN; IMMOBILIZATION;
COUNTERMEASURE
AB INTRODUCTION: Long-duration spaceflight results in a loss of muscle strength that poses both operational and medical risks, particularly during emergency egress, upon return to Earth, and during future extraterrestrial exploration. lsokinetic testing of the knee, ankle, and trunk quantifies movement-specific strength changes following spaceflight and offers insight into the effectiveness of in-flight exercise countermeasures.
METHODS: We retrospectively evaluated changes in isokinetic strength for 37 ISS crewmembers (Expeditions 1-25) following 163 38 d (mean +/- SD) of spaceflight. Gender, in-flight resistance exercise hardware, and preflight strength were examined as potential modifiers of spaceflight-induced strength changes.
RESULTS: Mean isokinetic strength declined 8-17% following spaceflight. One month after return to Earth, strength had improved, but small deficits of 1-9% persisted. Spaceflight-induced strength losses were not different between men and women. Mean strength losses were as much as 7% less in crewmembers who flew after the Advanced Resistive Exercise Device (ARED) replaced the interim Resistive Exercise Device (iRED) as the primary in-flight resistance exercise hardware, although these differences were not statistically significant. Absolute and relative preflight strength were moderately correlated (r = 0.47 and 0.54, respectively) with postflight strength changes.
DISCUSSION: In-flight resistance exercise did not prevent decreased isokinetic strength after long-duration spaceflight. However, continued utilization of ARED, a more robust resistance exercise device providing higher loads than iRED, may result in greater benefits as exercise prescriptions are optimized. With reconditioning upon return to Earth, strength is largely recovered within 30 d.
C1 [English, Kirk L.; Lee, Stuart M. C.; Loehr, James A.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Ploutz-Snyder, Robert J.; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX USA.
RP English, KL (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
NR 35
TC 4
Z9 4
U1 2
U2 5
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A68
EP A77
DI 10.3357/AMHP.EC09.2015
PG 10
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700009
PM 26630197
ER
PT J
AU Hayes, J
AF Hayes, Judith
TI The First Decade of ISS Exercise: Lessons Learned on Expeditions 1-25
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE exercise countermeasures; treadmill; resistance exercise; ergometer;
prescription
AB Long-duration spaceflight results in musculoskeletal, cardiorespiratory, and sensorimotor deconditioning. Historically, exercise has been used as a countermeasure to mitigate these deleterious effects that occur as a consequence of microgravity exposures. The International Space Station (ISS) exercise community describes their approaches, biomedical surveillance, and lessons learned in the development of exercise countermeasure modalities and prescriptions for maintaining health and performance among station crews. This report is focused on the first 10 yr of ISS defined as Expeditions 1-25 and includes only crewmembers with missions > 30 d on ISS for all 5 partner agencies (United States, Russia, Europe, Japan, and Canada). All 72 cosmonauts and astronauts participated in the ISS exercise countermeasures program. This Supplement presents a series of papers that provide an overview of the first decade of ISS exercise from a multidisciplinary, multinational perspective to evaluate the initial countermeasure program and record its operational limitations and challenges. In addition, we provide results from standardized medical evaluations before, during, and after each mission. Information presented in this context is intended to describe baseline conditions of the ISS exercise program. This paper offers an introduction to the subsequent series of manuscripts.
C1 [Hayes, Judith] NASA Johnson Space Ctr, Houston, TX USA.
RP Hayes, J (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU International Space Station (ISS)
FX No venture of this complexity could succeed without the contributions of
many. The supplement arose from a collaborative effort initiated by the
International Countermeasures Working Group and sponsored by the
International Space Station (ISS) partner agencies. Specifically, this
effort was supported by the following individuals and their affiliated
agencies: Patrik Sunblad (ESA European Space Research and Technology
Centre), Volker Damann (ESA European Astronaut Centre), Elena Fomina,
Eugenia Yarmonova and Inessa Kozlovskaya (Institut of Biomedical
Problems in Moscow), Natalie Hirsch (Canadian Space Agency) and Hiroshi
Ohshima (Japanese Aerospace Agency).
NR 8
TC 1
Z9 1
U1 1
U2 1
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A1
EP A6
DI 10.3357/AMHP.EC01.2015
PG 6
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700001
PM 26630187
ER
PT J
AU Korth, DW
AF Korth, Deborah W.
TI Exercise Countermeasure Hardware Evolution on ISS: The First Decade
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
AB The hardware systems necessary to support exercise countermeasures to the deconditioning associated with microgravity exposure have evolved and improved significantly during the first decade of the International Space Station (ISS), resulting in both new types of hardware and enhanced performance capabilities for initial hardware items. The original suite of countermeasure hardware supported the first crews to arrive on the ISS and the improved countermeasure system delivered in later missions continues to serve the astronauts today with increased efficacy. Due to aggressive hardware development schedules and constrained budgets, the initial approach was to identify existing spaceflight-certified exercise countermeasure equipment, when available, and modify it for use on the ISS. Program management encouraged the use of commercial-off-the-shelf (COTS) hardware, or hardware previously developed (heritage hardware) for the Space Shuttle Program. However, in many cases the resultant hardware did not meet the additional requirements necessary to support crew health maintenance during long-duration missions (3 to 12 mo) and anticipated future utilization activities in support of biomedical research. Hardware development was further complicated by performance requirements that were not fully defined at the outset and tended to evolve over the course of design and fabrication. Modifications, ranging from simple to extensive, were necessary to meet these evolving requirements in each case where heritage hardware was proposed. Heritage hardware was anticipated to be inherently reliable without the need for extensive ground testing, due to its prior positive history during operational spaceflight utilization. As a result, developmental budgets were typically insufficient and schedules were too constrained to permit long-term evaluation of dedicated ground-test units ("fleet leader" type testing) to identify reliability issues when applied to long-duration use. In most cases, the exercise unit with the most operational history was the unit installed on the ISS.
C1 [Korth, Deborah W.] NASA Johnson Space Ctr, Houston, TX USA.
RP Korth, DW (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
NR 2
TC 3
Z9 3
U1 0
U2 2
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A7
EP A13
DI 10.3357/AMHP.EC02.2015
PG 7
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700002
PM 26630190
ER
PT J
AU Kozlovskaya, IB
Yarmanova, EN
Yegorov, AD
Stepantsov, VI
Fomina, EV
Tomilovaskaya, ES
AF Kozlovskaya, Inessa B.
Yarmanova, E. N.
Yegorov, A. D.
Stepantsov, V. I.
Fomina, E. V.
Tomilovaskaya, E. S.
TI Russian Countermeasure Systems for Adverse Effects of Microgravity on
Long-Duration ISS Flights
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE spaceflight; human; history
ID TERM
AB The system of countermeasures for the adverse effects of microgravity developed in the USSR supported the successful implementation of long-duration spaceflight (LDS) programs on the Salyut and Mir orbital stations and was subsequently adapted for flights on the International Space Station (ISS). From 2000 through 2010, crews completed 26 ISS flight increments ranging in duration from 140 to 216 d, with the participation of 27 Russian cosmonauts. These flights have made it possible to more precisely determine a crewmember's level of conditioning, better assess the advantages and disadvantages of training processes, and determine prospects for future developments.
C1 [Kozlovskaya, Inessa B.; Yarmanova, E. N.; Yegorov, A. D.; Stepantsov, V. I.; Fomina, E. V.; Tomilovaskaya, E. S.] Moscow Biomed Problems Inst, Moscow, Russia.
RP Kozlovskaya, IB (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
RI Kozlovskaya, Inesa/R-9729-2016
FU Russian Science Foundation [14-25-00167]
FX This work was supported by Russian Science Foundation grant number:
14-25-00167.
NR 18
TC 3
Z9 3
U1 1
U2 4
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A24
EP A31
DI 10.3357/AMHP.EC04.2015
PG 8
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700004
PM 26630192
ER
PT J
AU Laughlin, MS
Guilliams, ME
Nieschwitz, BA
Hoellen, D
AF Laughlin, Mitzi S.
Guilliams, Mark E.
Nieschwitz, Bruce A.
Hoellen, David
TI Functional Fitness Testing Results Following Long-Duration ISS Missions
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE spaceflight; functional fitness test; rehabilitation
AB INTRODUCTION: Long-duration spaceflight missions lead to the loss of muscle strength and endurance. Significant reduction in muscle function can be hazardous when returning from spaceflight. To document these losses, NASA developed medical requirements that include measures of functional strength and endurance. Results from this Functional Fitness Test (FFT) battery are also used to evaluate the effectiveness of in-flight exercise countermeasures. The purpose of this paper is to document results from the FFT and correlate this information with performance of in-flight exercise on board the International Space Station.
METHODS: The FFT evaluates muscular strength and endurance, flexibility, and agility and includes the following eight measures: sit and reach, cone agility, push-ups, pull-ups, sliding crunches, bench press, leg press, and hand grip dynamometry. Pre- to postflight functional fitness measurements were analyzed using dependent t-tests and correlation analyses were used to evaluate the relationship between functional fitness measurements and in-flight exercise workouts.
RESULTS: Significant differences were noted postspaceflight with the sit and reach, cone agility, leg press, and hand grip measurements while other test scores were not significantly altered. The relationships between functional fitness and in-flight exercise measurements showed minimal to moderate correlations for most in-flight exercise training variables.
DISCUSSION: The change in FFT results can be partially explained by in-flight exercise performance. Although there are losses documented in the FFT results, it is important to realize that the crewmembers are successfully performing activities of daily living and are considered functional for normal activities upon return to Earth.
C1 [Laughlin, Mitzi S.; Guilliams, Mark E.; Nieschwitz, Bruce A.; Hoellen, David] Wyle Sci Technol & Engn Grp, Houston, TX USA.
RP Laughlin, MS (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260 - ISS medical Operations Requirements Document (MORD) and
SSP 50667- Medical Evaluations Documentation (MED) Volume B. This
article would not have been possible without a great deal of help from
many people. We would like to thank all former Astronaut Strength,
Conditioning, and Rehabilitation specialists (ASCRs), as this article
includes 10 years of ISS data, and without their dedication and
professionalism this would never had been possible. We are greatly
indebted to Beth Shephard, Jamie Chauvin, Corey Twine, Yamil Garcia,
Bill Amonette, Christi Baker, and Stephanie Fox. Additionally, Roxanne
Buxton and Peggy Lynn have processed the in-flight exercise data for the
last few years and we wish to thank you.
NR 8
TC 1
Z9 1
U1 1
U2 2
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A87
EP A91
DI 10.3357/AMHP.EC11.2015
PG 5
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700011
PM 26630199
ER
PT J
AU Lee, SMC
Feiveson, AH
Stein, S
Stenger, MB
Platts, SH
AF Lee, Stuart M. C.
Feiveson, Alan H.
Stein, Sydney
Stenger, Michael B.
Platts, Steven H.
TI Orthostatic Intolerance After ISS and Space Shuttle Missions
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE Tilt test; Space Shuttle; tilt survival
ID BED-REST; COMPRESSION GARMENTS; RESISTANCE EXERCISE; STAND-TEST;
SPACEFLIGHT; TOLERANCE; COUNTERMEASURE; VOLUME; RESPONSES; PRESSURE
AB INTRODUCTION: Cardiovascular deconditioning apparently progresses with flight duration, resulting in a greater incidence of orthostatic intolerance following long-duration missions, Therefore, we anticipated that the proportion of astronauts who could not complete an orthostatic tilt test (OTT) would be higher on landing day and the number of days to recover greater after International Space Station (ISS) than after Space Shuttle missions.
METHODS: There were 20 ISS and 65 Shuttle astronauts who participated in 10-min 800 degrees head-up tilt tests 10 d before launch, on landing day (R+0), and 3d after landing (R+3). Fisher's ExactTest was used to compare the ability of ISS and Shuttle astronauts to complete the OTT. Cox regression was used to identify cardiovascular parameters associated with OTT completion and mixed model analysis was used to compare the change and recovery rates between groups.
RESULTS: The proportion of astronauts who completed the OTT on R+0 (2 of 6) was less in ISS than in Shuttle astronauts (52 of 65). On R+3, 13 of 15 and 19 of 19 of the ISS and Shuttle astronauts, respectively, completed the OTT. An index comprised of stroke volume and diastolic blood pressure provided a good prediction of OTT completion and was altered by spaceflight similarly for both astronaut groups, but recovery was slower in ISS than in Shuttle astronauts.
CONCLUSIONS: The proportion of ISS astronauts who could not complete the OTT on R+0 was greater and the recovery rate slower after ISS compared to Shuttle missions. Thus, mission planners and crew surgeons should anticipate the need to tailor scheduled activities and level of medical support to accommodate protracted recovery after long-duration microgravity exposures.
C1 [Lee, Stuart M. C.; Stenger, Michael B.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Feiveson, Alan H.; Platts, Steven H.] NASA Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX USA.
[Stein, Sydney] MEI Technol, Houston, TX USA.
RP Lee, SMC (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260 - ISS Medical Operations Requirements Document (MORD) and
SSP 50667 - Medical Evaluations Documentation (MED) Volume B. The
authors wish to thank the astronauts for their participation in these
tests; the staff of the JSC's Cardiovascular Laboratory for the
collection and reduction of the tilt test data; the JSC Bone and Mineral
Laboratory and the Exercise Physiology Laboratory for sharing the lean
tissue mass and cycle ergometer test data, respectively; the Mission
Integration Coordinators who coordinated the test schedule and assisted
with some aspects of tilt data collection; the Lifetime Surveillance of
Astronaut Health Program for their assistance with some data sets; and
Dr. Charles Sawin and the special edition editorial staff for their
helpful guidance.
NR 47
TC 4
Z9 4
U1 0
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A54
EP A67
DI 10.3357/AMHP.EC08.2015
PG 14
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700008
PM 26630196
ER
PT J
AU Loehr, JA
Guilliams, ME
Petersen, N
Hirsch, N
Kawashima, S
Ohshima, H
AF Loehr, James A.
Guilliams, Mark E.
Petersen, Nora
Hirsch, Natalie
Kawashima, Shino
Ohshima, Hiroshi
TI Physical Training for Long-Duration Spaceflight
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE physiologic deconditioning; exercise training
AB Physical training has been conducted on the International Space Station (ISS) for the past 10 yr as a countermeasure to physiological deconditioning during spaceflight. Each member space agency has developed its own approach to creating and implementing physical training protocols for their astronauts. We have divided physical training into three distinct phases (preflight, in-flight, and postflight) and provided a description of each phase with its constraints and limitations. We also discuss how each member agency (NASA, ESA, CSA, and JAXA) prescribed physical training for their crewmembers during the first 10 yr of ISS operations. It is important to understand the operational environment, the agency responsible for the physical training program, and the constraints and limitations associated with spaceflight to accurately design and implement exercise training or interpret the exercise data collected on ISS. As exploration missions move forward, resolving agency differences in physical training programs will become important to maximizing the effectiveness of exercise as a countermeasure and minimizing any mission impacts.
C1 [Loehr, James A.; Guilliams, Mark E.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Petersen, Nora] Wyle Labs GmbH, European Space Agcy Space Med Off, Cologne, Germany.
[Hirsch, Natalie] Canadian Space Agcy, St Hubert, PQ, Canada.
[Kawashima, Shino] Adv Engn Serv Co Ltd, Tsukuba, Ibaraki, Japan.
[Ohshima, Hiroshi] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.
RP Loehr, JA (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260 - ISS Medical Operations Requirements Document (MORD) and
SSP 50667 - Medical Evaluations Documentation (MED) Volume B.
NR 4
TC 8
Z9 8
U1 2
U2 4
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A14
EP A23
DI 10.3357/AMHP.EC03.2015
PG 10
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700003
PM 26630191
ER
PT J
AU Loerch, LH
AF Loerch, Linda H.
TI Exercise Countermeasures on ISS: Summary and Future Directions
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE Microgravity; exercise countermeasures
AB The first decade of the International Space Station Program (ISS) yielded a wealth of knowledge regarding the health and performance of crewmembers living in microgravity for extended periods of time. The exercise countermeasures hardware suite evolved during the last decade to provide enhanced capabilities that were previously unavailable to support human spaceflight, resulting in attenuation of cardiovascular, muscle, and bone deconditioning. The ability to protect crew and complete mission tasks in the autonomous exploration environment will be a critical component of any decision to proceed with manned exploration initiatives. The next decade of ISS habitation promises to be a period of great scientific utilization that will yield both the tools and technologies required to safely explore the solar system. Leading countermeasure candidates for exploration class missions must be studied methodically on ISS over the next decade to ensure protocols and systems are highly efficient, effective, and validated. Lessons learned from the ISS experience to date are being applied to the future, and international cooperation enables us to maximize this exceptional research laboratory.
C1 [Loerch, Linda H.] NASA Johnson Space Ctr, Houston, TX USA.
RP Loerch, LH (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
NR 0
TC 2
Z9 2
U1 1
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A92
EP A93
DI 10.3357/AMHP.EC12.2015
PG 2
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700012
PM 26630200
ER
PT J
AU Moore, AD
Lynn, PA
Feiveson, AH
AF Moore, Alan D., Jr.
Lynn, Peggy A.
Feiveson, Alan H.
TI The First 10 Years of Aerobic Exercise Responses to Long-Duration 155
Flights
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE spaceflight; aerobic capacity; exercise
ID MANNED SKYLAB MISSION; DOWN BED REST; ORTHOSTATIC INTOLERANCE; CARDIAC
ATROPHY; CARDIOVASCULAR RISKS; SUBMAXIMAL EXERCISE; MAXIMAL EXERCISE;
EXPERIMENT M-171; SPACE-FLIGHTS; SPACEFLIGHT
AB INTRODUCTION: Aerobic deconditioning may occur during International Space Station (ISS) flights. This paper documents findings from exercise testing conducted before, during, and after ISS expeditions.
METHODS: There were 30 male and 7 female astronauts on ISS missions (48 to 219 d, mean 163 d) who performed cycle exercise protocols consisting of 5-min stages eliciting 25%, 50%, and 75% peak oxygen uptake (Vo(2peak)) Tests were conducted 30 to 90 d before missions, on flight day 15 and every 30 flight days thereafter, and on recovery (R) days +5 and +30. During pre- and postflight tests, heart rate (HR) and metabolic gas exchange were measured. During flight, extrapolation of the HR and Vo(2) relationship to preflight-measured peak HR provided an estimate of Vo2peak, referred to as the aerobic capacity index (ACI).
RESULTS: HR during each exercise stage was elevated (P < 0.05) and oxygen pulse was reduced (P < 0.05) on R+5 compared to preflight; however, no other metabolic gas analysis values significantly changed. Compared to preflight, the ACI declined (P < 0.001) on R+5, but recovered to levels greater than preflight by R+30 (P = 0.008). During flight, ACI decreased below preflight values, but increased with mission duration (P < 0.001).
CONCLUSIONS: Aerobic deconditioning likely occurs initially during flight, but ACI recovers toward preflight levels as flight duration increases, presumably due to performance of exercise countermeasures. Elevated HR and lowered oxygen pulse on R+5 likely results from some combination of relative hypovolemia, lowered cardiac stroke volume, reduced cardiac distensibility, and anemia, but recovery occurs by R+30.
C1 [Moore, Alan D., Jr.] Lamar Univ, Dept Hlth & Kinesiol, Beaumont, TX 77710 USA.
[Lynn, Peggy A.] Wyle Sci Technol & Engn Business Grp, Houston, TX USA.
[Feiveson, Alan H.] NASA Johnson Space Ctr, Houston, TX USA.
RP Moore, AD (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260 - ISS medical Operations Requirements Document (MORD) and
SSP 50667 - Medical Evaluations Documentation (MED) Volume B. The
authors wish to thank the members of the NASA Exercise Countermeasures
Project and many of the team members of the NASA Human Health and
Performance Directorate at the Johnson Space Center for their support of
this manuscript. Specific recognition is deserved for those involved in
the aerobic exercise data collection over the first 10 years of ISS
flight. These outstanding individuals are: Stuart Lee, Meghan Everett,
Jamie Guined, Mark Leach, Kirk English, Roxanne Buxton, Elizabeth
Goetchius, Jason Wicicwire, Brent Crowell, Frank McCleary, James Loehr,
W Jon Williams, Jason Norcross, Cassie Wilson, and Kristi Blazine.
NR 42
TC 2
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U1 0
U2 2
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A78
EP A86
DI 10.3357/AMHP.EC10.2015
PG 9
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700010
PM 26630198
ER
PT J
AU Sibonga, JD
Spector, ER
Johnston, SL
Tarver, WJ
AF Sibonga, Jean D.
Spector, Elisabeth R.
Johnston, Smith L.
Tarver, William J.
TI Evaluating Bone Loss in ISS Astronauts
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE densitometry; bone mineral density; trabecular bone; cortical bone
ID LONG-DURATION SPACEFLIGHT; QUANTITATIVE COMPUTED-TOMOGRAPHY; PROXIMAL
FEMUR; HIP FRACTURE; OSTEOPOROTIC FRACTURES; MINERAL DENSITY; STRENGTH;
WOMEN; DETERMINANTS; PREVENTION
AB The measurement of bone mineral density (BMD) by dual-energy X-ray absorptiometry (DXA) is the Medical Assessment Test used at the NASA Johnson Space Center to evaluate whether prolonged exposure to spaceflight increases the risk for premature osteoporosis in International Space Station (ISS) astronauts. The DXA scans of crewmembers'BMD during the first decade of the ISS existence showed precipitous declines in BMD for the hip and spine after the typical 6-mo missions. However, a concern exists that skeletal integrity cannot be sufficiently assessed solely by DXA measurement of BMD. Consequently, use of relatively new research technologies is being proposed to NASA for risk surveillance and to enhance long-term management of skeletal health in long-duration astronauts.
C1 [Sibonga, Jean D.; Johnston, Smith L.; Tarver, William J.] NASA Johnson Space Ctr, Houston, TX USA.
[Spector, Elisabeth R.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
RP Sibonga, JD (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260-ISS Medical Operations Requirements Document (MORD) and SSP
50667-Medical Evaluations Documentation (MED) Volume B. The authors wish
to thank members of the Balance Control Laboratory at NASA Johnson Space
Center for data collection and analysis support, the mission integration
coordinators for implementation support, and the flight surgeons who
advocated for the continued use of DXA as a medical requirement.
Finally, we thank the crewmember participants for their willing
participation and insightful feedback.
NR 34
TC 1
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U1 3
U2 13
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A38
EP A44
DI 10.3357/AMHP.EC06.2015
PG 7
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700006
PM 26630194
ER
PT J
AU Wood, SJ
Paloski, WH
Clark, JB
AF Wood, Scott J.
Paloski, William H.
Clark, Jonathan B.
TI Assessing Sensorimotor Function Following ISS with Computerized Dynamic
Posturography
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE ataxia; vestibular; ISS; postflight; multisensory; unloading
ID DURATION SPACEFLIGHT; SPATIAL ORIENTATION; MOTION SICKNESS;
SPACE-STATION; MICROGRAVITY; WEIGHTLESSNESS; BALANCE; MUSCLE;
READAPTATION; ADAPTATION
AB INTRODUCTION: Postflight postural ataxia reflects both the control strategies adopted for movement in microgravity and the direct effects of deconditioning. Computerized dynamic posturography (CDP) has been used during the first decade of the International Space Station (ISS) expeditions to quantify the initial postflight decrements and recovery of postural stability.
METHODS: The CDP data were obtained on 37 crewmembers as part of their pre- and postflight medical examinations. Sensory organization tests evaluated the ability to make effective use of (or suppress inappropriate) visual, vestibular, and somatosensory information for balance control. This report focuses on eyes closed conditions with either a fixed or sway-referenced base of support, with the head erect or during pitch-head tilts (+/- 20 degrees at 0.33 Hz). Equilibrium scores were derived from peak-to-peak anterior-posterior sway. Motor-control tests were also used to evaluate a crewmember's ability to automatically recover from unexpected support-surface perturbations.
RESULTS: The standard Romberg condition was the least sensitive. Dynamic head tilts led to increased incidence of falls and revealed significantly longer recovery than head-erect conditions. Improvements in postflight postural performance during the later expeditions may be attributable to higher preflight baselines and/or advanced exercise capabilities aboard the ISS.
CONCLUSIONS: The diagnostic assessment of postural instability is more pronounced during unstable-support conditions requiring active head movements. In addition to supporting return-to-duty decisions by flight surgeons, the CDP provides a standardized sensorimotor measure that can be used to evaluate the effectiveness of countermeasures designed to either minimize deconditioning on orbit or promote reconditioning upon return to Earth.
C1 [Wood, Scott J.] Azusa Pacific Univ, Azusa, CA USA.
[Paloski, William H.] NASA Johnson Space Ctr, Houston, TX USA.
[Clark, Jonathan B.] Baylor Coll Med, Ctr Space Med, Houston, TX 77030 USA.
RP Wood, SJ (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
FU NASA ISS Program Office [SSP 50260, SSP 50667]
FX This report was sponsored by the NASA ISS Program Office with reference
to SSP 50260 - ISS Medical Operations Requirements Document (MORD) and
SSP 50667 - Medical Evaluations Documentation (MED) Volume B. The
authors wish to thank members of the Balance Control Laboratory at NASA
Johnson Space Center for data collection and analysis support, the
mission integration coordinators for implementation support, and the
flight surgeons who advocated for the continued use of CDP as a medical
requirement. Finally, we thank the crewmember participants for their
willing participation and insightful feedback
NR 42
TC 3
Z9 3
U1 0
U2 2
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A45
EP A53
DI 10.3357/AMHP.EC07.2015
PG 9
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700007
PM 26630195
ER
PT J
AU Yarmanova, EN
Kozlovskaya, IB
Khimoroda, NN
Fomina, EV
AF Yarmanova, Eugenia N.
Kozlovskaya, Inessa B.
Khimoroda, N. N.
Fomina, Elena V.
TI Evolution of Russian Microgravity Countermeasures
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE microgravity; International Space Station; exercise; treadmill; cycle
ergometer; LBNP; resistance bands; muscle loading; fluid loading
ID TERM
AB Countermeasures to prevent or partially offset the negative physiologic changes that are caused by the effects of microgravity play an important role in supporting the performance of crewmembers in flight and their safe return to Earth. Research conducted in Russia on the orbital stations Salyut and Mir, as well as simulation experiments on the ground, have demonstrated that changes that occur during extended spaceflight in various physiologic systems can be prevented or significantly decreased by using countermeasures. Hardware and techniques used on the ISS have been substantially improved to reflect the experience of previous extended missions on Russian orbital stations. Countermeasures used during early ISS missions consisted of the U.S. treadmill (TVIS), cycle ergometer (BB-3), a set of resistance bands, a postural muscle loading suit (Penguin-3), electrical stimulator (Tonus-3), compression thigh cuffs (Braslet-M), a lower body negative pressure (LBNP) suit (Chibis), a lower body g-loading suit (Kentavr), and water/salt supplements. These countermeasures are described in this article.
C1 [Yarmanova, Eugenia N.; Kozlovskaya, Inessa B.; Khimoroda, N. N.; Fomina, Elena V.] Moscow Biomed Problems Inst, Moscow, Russia.
RP Yarmanova, EN (reprint author), Care Of Reeves JM, NASA Johnson Space Ctr, Div Resource Support, Biomed Res & Environm Sci Div, 2101 NASA Pkwy,MC Wyle SK-37, Houston, TX 77058 USA.
EM Jacqueline.m.reeves@nasa.gov
RI Kozlovskaya, Inesa/R-9729-2016
FU Russian Science Foundation [14-25-00167]
FX This work was supported by Russian Science Foundation grant number:
14-25-00167.
NR 9
TC 0
Z9 0
U1 4
U2 6
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD DEC
PY 2015
VL 86
IS 12
SU S
BP A32
EP A37
DI 10.3357/AMHP.EC05.2015
PG 6
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CX6VB
UT WOS:000365838700005
PM 26630193
ER
PT J
AU Loikith, PC
Waliser, DE
Lee, H
Neelin, JD
Lintner, BR
McGinnis, S
Mearns, LO
Kim, J
AF Loikith, Paul C.
Waliser, Duane E.
Lee, Huikyo
Neelin, J. David
Lintner, Benjamin R.
McGinnis, Seth
Mearns, Linda O.
Kim, Jinwon
TI Evaluation of large-scale meteorological patterns associated with
temperature extremes in the NARCCAP regional climate model simulations
SO CLIMATE DYNAMICS
LA English
DT Article
DE Temperature extremes; Regional climate modeling; Large-scale
meteorological patterns; North America; Model evaluation
ID NORTH-AMERICA; UNITED-STATES; HEAT WAVES; ATMOSPHERE INTERACTIONS;
SOIL-MOISTURE; COUPLED MODEL; CIRCULATION; VARIABILITY; REANALYSIS;
IMPACT
AB Large-scale meteorological patterns (LSMPs) associated with temperature extremes are evaluated in a suite of regional climate model (RCM) simulations contributing to the North American Regional Climate Change Assessment Program. LSMPs are characterized through composites of surface air temperature, sea level pressure, and 500 hPa geopotential height anomalies concurrent with extreme temperature days. Six of the seventeen RCM simulations are driven by boundary conditions from reanalysis while the other eleven are driven by one of four global climate models (GCMs). Four illustrative case studies are analyzed in detail. Model fidelity in LSMP spatial representation is high for cold winter extremes near Chicago. Winter warm extremes are captured by most RCMs in northern California, with some notable exceptions. Model fidelity is lower for cool summer days near Houston and extreme summer heat events in the Ohio Valley. Physical interpretation of these patterns and identification of well-simulated cases, such as for Chicago, boosts confidence in the ability of these models to simulate days in the tails of the temperature distribution. Results appear consistent with the expectation that the ability of an RCM to reproduce a realistically shaped frequency distribution for temperature, especially at the tails, is related to its fidelity in simulating LMSPs. Each ensemble member is ranked for its ability to reproduce LSMPs associated with observed warm and cold extremes, identifying systematically high performing RCMs and the GCMs that provide superior boundary forcing. The methodology developed here provides a framework for identifying regions where further process-based evaluation would improve the understanding of simulation error and help guide future model improvement and downscaling efforts.
C1 [Loikith, Paul C.; Waliser, Duane E.; Lee, Huikyo] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Waliser, Duane E.; Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Lintner, Benjamin R.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[McGinnis, Seth; Mearns, Linda O.] Natl Ctr Atmospher Res, Inst Math Applicat Geosci, Boulder, CO 80307 USA.
RP Loikith, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA.
EM paul.c.loikith@jpl.nasa.gov
OI McGinnis, Seth/0000-0001-8082-834X
FU NASA National Climate Assessment [11-NCA11-0028]; NSF [AGS-1102838]
FX Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Part of this research was funded
by NASA National Climate Assessment 11-NCA11-0028 (P.C.L., J.K., H.L.,
D.E.W) and NSF AGS-1102838 (J.D.N.). We also thank the NARCCAP team for
production of the model simulations and archiving of the data. We thank
Joyce Meyerson for her valuable contributions to figure production.
NR 63
TC 3
Z9 3
U1 5
U2 19
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD DEC
PY 2015
VL 45
IS 11-12
BP 3257
EP 3274
DI 10.1007/s00382-015-2537-x
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX0WU
UT WOS:000365418900019
ER
PT J
AU Wright, DB
Knutson, TR
Smith, JA
AF Wright, Daniel B.
Knutson, Thomas R.
Smith, James A.
TI Regional climate model projections of rainfall from US landfalling
tropical cyclones
SO CLIMATE DYNAMICS
LA English
DT Article
DE Tropical cyclones; Extreme rainfall; Floods; Climate impacts; Climate
modeling; Dynamical downscaling
ID STOCHASTIC STORM TRANSPOSITION; EXTRATROPICAL TRANSITION; UNITED-STATES;
INTENSE PRECIPITATION; CMIP5 MODELS; PART I; FREQUENCY; TRMM;
HURRICANES; EVOLUTION
AB The eastern United States is vulnerable to flooding from tropical cyclone rainfall. Understanding how both the frequency and intensity of this rainfall will change in the future climate is a major challenge. One promising approach is the dynamical downscaling of relatively coarse general circulation model results using higher-resolution regional climate models (RCMs). In this paper, we examine the frequency of landfalling tropical cyclones and associated rainfall properties over the eastern United States using Zetac, an 18-km resolution RCM designed for modeling Atlantic tropical cyclone activity. Simulations of 1980-2006 tropical cyclone frequency and rainfall intensity for the months of August-October are compared against results from previous studies and observation-based datasets. The 1980-2006 control simulations are then compared against results from three future climate scenarios: CMIP3/A1B (late twenty-first century) and CMIP5/RCP4.5 (early and late twenty-first century). In CMIP5 early and late twenty-first century projections, the frequency of occurrence of post-landfall tropical cyclones shows little net change over much of the eastern U.S. despite a decrease in frequency over the ocean. This reflects a greater landfalling fraction in CMIP5 projections, which is not seen in CMIP3-based projections. Average tropical cyclone rain rates over land within 500 km of the storm center increase by 8-17 % in the future climate projections relative to control. This is at least as much as expected from the Clausius-Clapeyron relation, which links a warmer atmosphere to greater atmospheric water vapor content. Over land, the percent enhancement of area-averaged rain rates from a given tropical cyclone in the warmer climate is greater for larger averaging radius (300-500 km) than near the storm, particularly for the CMIP3 projections. Although this study does not focus on attribution, the findings are broadly consistent with historical tropical cyclone rainfall changes documented in a recent observational study. The results may have important implications for future flood risks from tropical cyclones.
C1 [Wright, Daniel B.] NASA Hydrol Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wright, Daniel B.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Knutson, Thomas R.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA.
[Smith, James A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
RP Wright, DB (reprint author), NASA Hydrol Sci, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM daniel.b.wright@nasa.gov
FU Willis Research Network; National Oceanic and Atmospheric Administration
Cooperative Institute for Climate Sciences [NOAA CICS NA08OAR4320752];
National Science Foundation [CBET-1058027]; NASA Postdoctoral Program
FX This work was partially funded by the Willis Research Network, the
National Oceanic and Atmospheric Administration Cooperative Institute
for Climate Sciences (Grant NOAA CICS NA08OAR4320752), and the the
National Science Foundation (Grant CBET-1058027) and the NASA
Postdoctoral Program. We would like to thank Joseph Sirutis of NOAA GFDL
for providing climate model data, Joshua Roundy of Princeton University
and NASA GSFC for preparing the NLDAS rainfall data, and Timothy Marchok
and Baoqiang Xiang of NOAA GFDL for their thoughtful comments.
NR 64
TC 1
Z9 1
U1 5
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD DEC
PY 2015
VL 45
IS 11-12
BP 3365
EP 3379
DI 10.1007/s00382-015-2544-y
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX0WU
UT WOS:000365418900025
ER
PT J
AU Miller, KB
Huettmann, F
Norcross, BL
AF Miller, K. B.
Huettmann, F.
Norcross, B. L.
TI Efficient spatial models for predicting the occurrence of subarctic
estuarine-associated fishes: implications for management
SO FISHERIES MANAGEMENT AND ECOLOGY
LA English
DT Article
DE essential fish habitat; estuaries; fisheries management; random forest;
species distribution models
ID SPECIES DISTRIBUTION MODELS; SOUTHEAST ALASKA; RANDOM FORESTS; REEF
FISHES; HABITAT; DISTRIBUTIONS; ATLANTIC; PATTERNS; CONSERVATION;
REGRESSION
AB In many of the nearshore areas where development is most likely to occur, essential fish habitat data are incomplete and there is little information on species occurrence that can be used to inform management decisions. This research investigated the use of multivariate remotely sensed geomorphic and landscape data to develop accurate predictive models of subarctic, estuarine-associated fishes. The random forest algorithm was used to predict the occurrence of 26 fish species captured in 49 estuaries in Southeast Alaska. Model prediction accuracy ranged from 100 to 42% for species presence and 87 to 15% for species absence. Model goodness of fit and accuracy were assessed by comparing the number of species occurrences predicted by the model against the observed presences and absences of species in an independent data set. Sixty percent of the models were able to predict species presence with an accuracy of 70% or better. The models were used to predict species occurrence for 521 unsampled Southeast Alaskan estuaries to provide a regional map of predicted species distributions.
C1 [Miller, K. B.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
[Huettmann, F.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Inst Arctic Biol, EWHALE Lab, Fairbanks, AK USA.
[Norcross, B. L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK USA.
RP Miller, KB (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
EM katharine.miller@noaa.gov
NR 69
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0969-997X
EI 1365-2400
J9 FISHERIES MANAG ECOL
JI Fisheries Manag. Ecol.
PD DEC
PY 2015
VL 22
IS 6
BP 501
EP 517
DI 10.1111/fme.12148
PG 17
WC Fisheries
SC Fisheries
GA CX5CL
UT WOS:000365718900006
ER
PT J
AU Orbe, C
Newman, PA
Waugh, DW
Holzer, M
Oman, LD
Li, F
Polvani, LM
AF Orbe, Clara
Newman, Paul A.
Waugh, Darryn W.
Holzer, Mark
Oman, Luke D.
Li, Feng
Polvani, Lorenzo M.
TI Air-mass Origin in the Arctic. Part II: Response to Increases in
Greenhouse Gases
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Geographic location; entity; Arctic; Circulation; Dynamics; Transport;
Models and modeling; Climate models; Tracers
ID SEA-ICE COVER; CLIMATE; TRANSPORT; CIRCULATION; TRENDS; VARIABILITY;
POLLUTION; OCEAN; NAO
AB Future changes in transport from Northern Hemisphere (NH) midlatitudes into the Arctic are examined using rigorously defined air-mass fractions that partition air in the Arctic according to where it last had contact with the planetary boundary layer (PBL). Boreal winter (December-February) and summer (June-August) air-mass fraction climatologies are calculated for the modeled climate of the Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM) forced with the end-of-twenty-first century greenhouse gases and ozone-depleting substances. The modeled projections indicate that the fraction of air in the Arctic that last contacted the PBL over NH midlatitudes (or air of midlatitude origin) will increase by about 10% in both winter and summer. The projected increases during winter are largest in the upper and middle Arctic troposphere, where they reflect an upward and poleward shift in the transient eddy meridional wind, a robust dynamical response among comprehensive climate models. The boreal winter response is dominated by (similar to 5%-10%) increases in the air-mass fractions originating over the eastern Pacific and the Atlantic, while the response in boreal summer mainly reflects (similar to 5%) increases in air of Asian and North American origin. The results herein suggest that future changes in transport from midlatitudes may impact the compositionand, hence, radiative budgetin the Arctic, independent of changes in emissions.
C1 [Orbe, Clara; Newman, Paul A.; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Holzer, Mark] Univ New S Wales, Sch Math & Stat, Dept Appl Math, Sydney, NSW, Australia.
[Holzer, Mark; Polvani, Lorenzo M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Li, Feng] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Polvani, Lorenzo M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
EM clara.orbe@nasa.gov
RI Oman, Luke/C-2778-2009; Waugh, Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; Waugh, Darryn/0000-0001-7692-2798
FU ARC [DP120100674]; NSF [AGS-1403676, AGS-1402931]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The authors also
acknowledge support from ARC Grant DP120100674 (M.H.) and NSF Grants
AGS-1403676 (D.W.) and AGS-1402931 (M.H., L.M.P.).
NR 36
TC 2
Z9 2
U1 2
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD DEC
PY 2015
VL 28
IS 23
BP 9105
EP 9120
DI 10.1175/JCLI-D-15-0296.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX7DC
UT WOS:000365860500004
ER
PT J
AU Yu, JY
Paek, H
Saltzman, ES
Lee, T
AF Yu, Jin-Yi
Paek, Houk
Saltzman, Eric S.
Lee, Tong
TI The Early 1990s Change in ENSO-PSA-SAM Relationships and Its Impact on
Southern Hemisphere Climate
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Geographic location; entity; Antarctica; Sea ice; Circulation; Dynamics;
Antarctic Oscillation; ENSO; Teleconnections; Variability; Interannual
variability
ID SEA-SURFACE TEMPERATURE; ZONAL FLOW VACILLATION; TROPICAL INDIAN-OCEAN;
ANNULAR MODE; EL-NINO; ATMOSPHERIC CIRCULATION; AMERICAN MODES;
VARIABILITY; PACIFIC; OSCILLATION
AB This study uncovers an early 1990s change in the relationships between El Nino-Southern Oscillation (ENSO) and two leading modes of the Southern Hemisphere (SH) atmospheric variability: the southern annular mode (SAM) and the Pacific-South American (PSA) pattern. During austral spring, while the PSA maintained a strong correlation with ENSO throughout the period 1948-2014, the SAM-ENSO correlation changed from being weak before the early 1990s to being strong afterward. Through the ENSO connection, PSA and SAM became more in-phase correlated after the early 1990s. The early 1990s is also the time when ENSO changed from being dominated by the eastern Pacific (EP) type to being dominated by the central Pacific (CP) type. Analyses show that, while the EP ENSO can excite only the PSA, the CP ENSO can excite both the SAM and PSA through tropospheric and stratospheric pathway mechanisms. The more in-phase relationship between SAM and PSA impacted the post-1990s Antarctic climate in at least two aspects: 1) a stronger Antarctic sea ice dipole structure around the Amundsen-Bellingshausen Seas due to intensified geopotential height anomalies over the region and 2) a shift in the phase relationships of surface air temperature anomalies among East Antarctica, West Antarctica, and the Antarctic Peninsula. These findings imply that ENSO-Antarctic climate relations depend on the dominant ENSO type and that ENSO forcing has become more important to the Antarctic sea ice and surface air temperature variability in the past two decades and will in the coming decades if the dominance of CP ENSO persists.
C1 [Yu, Jin-Yi; Paek, Houk; Saltzman, Eric S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yu, JY (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, 3200 Croul Hall St, Irvine, CA 92697 USA.
EM jyyu@uci.edu
RI Paek, Houk/L-6348-2016
OI Paek, Houk/0000-0002-4284-0660
FU NSF's Climate and Large-scale Dynamics Program [AGS-1233542,
AGS-1505145]
FX The authors thank two anonymous reviewers and Editor John Walsh for
their very constructive comments that have helped improve the paper.
This research was supported by NSF's Climate and Large-scale Dynamics
Program under Grants AGS-1233542 and AGS-1505145. The effort by Tong Lee
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. The NCEP-NCAR reanalysis data were obtained at
www.esrl.noaa.gov/psd, HadISST data are available at
www.metoffice.gov.uk/hadobs/hadisst, and the SAM* index data are
available at http://www.nerc-bas.ac.uk/icd/gjma/sam.html.
NR 61
TC 6
Z9 7
U1 0
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD DEC
PY 2015
VL 28
IS 23
BP 9393
EP 9408
DI 10.1175/JCLI-D-15-0335.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX7DC
UT WOS:000365860500020
ER
PT J
AU Wang, YH
Liu, WT
AF Wang, Yi-Hui
Liu, W. Timothy
TI Observational Evidence of Frontal-Scale Atmospheric Responses to
Kuroshio Extension Variability
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Circulation; Dynamics; Atmosphere-ocean interaction; Boundary currents;
Atm; Ocean Structure; Phenomena; Marine boundary layer; Troposphere;
Observational techniques and algorithms; Satellite observations
ID SEA-SURFACE TEMPERATURE; EASTERN EQUATORIAL PACIFIC; PLANETARY
BOUNDARY-LAYER; GULF-STREAM; SATELLITE-OBSERVATIONS; OCEAN; SST;
REANALYSIS; CLIMATOLOGY; PERFORMANCE
AB This study investigates the regional atmospheric response to the Kuroshio Extension (KE) using a combination of multiple satellite observations and reanalysis data from boreal winter over a period of at least a decade. The goal is to understand the relationship between KE variations and atmospheric responses at low frequencies. A climate index is used to measure the interannual to decadal KE variability, which leaves remarkable imprints on the mesoscale sea surface temperature (SST). Clear spatial coherence between the SST signals and frontal-scale atmospheric variables, including surface wind convergence, vertical velocity, precipitation, and clouds, is identified by linear regression analysis. Consistent with previous studies, the penetrating effect of the KE variability on the free atmosphere is found. The westward tilt of the atmospheric response above the KE near 500 hPa is revealed. The difference in the associations of frontal-scale air temperature and geopotential height with the KE variability between the satellite observations and the reanalysis data suggests an imperfect interpretation of frontal-scale oceanic forcing on the overlying atmosphere in the reanalysis assimilation system.
C1 [Wang, Yi-Hui; Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wang, YH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yi-hui.wang@jpl.nasa.gov
FU NASA
FX This work was supported by an appointment to the National Aeronautics
and Space Administration (NASA) Postdoctoral Program at the Jet
Propulsion Laboratory, California Institute of Techonology, administered
by Oak Ridge Associated Universities through a contract with the NASA.
Dr. W. T. Liu was supported jointly by the NASA Physical Oceanography
Program, Precipitation Measuring Mission, and Energy and Water Cycle
Studies. Dr. Xiaosu Xie kindly provided information on filtering and
data access. Dr. Jui-Lin (Frank) Li shared useful comments on the
results.
NR 37
TC 1
Z9 1
U1 3
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD DEC
PY 2015
VL 28
IS 23
BP 9459
EP 9472
DI 10.1175/JCLI-D-14-00829.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX7DC
UT WOS:000365860500024
ER
PT J
AU Weaver, C
Herman, J
Labow, G
Larko, D
Huang, LK
AF Weaver, Clark
Herman, Jay
Labow, Gordon
Larko, David
Huang, L. -K.
TI Shortwave TOA Cloud Radiative Forcing Derived from a Long-Term
(1980-Present) Record of Satellite UV Reflectivity and CERES
Measurements
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Physical Meteorology and Climatology; Cloud forcing
ID ENERGY SYSTEM CERES; OZONE DATA; EARTHS; CALIBRATION; ALGORITHM; TOMS;
NM
AB A 34-yr record of shortwave top-of-atmosphere (TOA) radiative cloud forcing is derived from UV Lambertian equivalent reflectivity (LER) data constructed using measured upwelling radiances from the Nimbus-7 Solar Backscatter Ultraviolet (SBUV) and from seven NOAA SBUV/2 instruments on polar-orbiting satellites. The approach is to scale the dimensionless UV LER data to match the CERES shortwave cloud radiative forcing when they are concurrent (2000-13). The underlying trends of this new longer-term CERES-like data record are solely based on the UV LER record. The good agreement between trends and anomalies of the CERES-like and CERES shortwave cloud forcing records during the overlapping data period supports using this new dataset for extended climate studies. The estimated linear trend for the shortwave TOA radiative forcing due to clouds from 60 degrees S to 60 degrees N is +1.47 W m(-2) with a 0.11 uncertainty at the 95% confidence level over the 34-yr period 1980-2013.
C1 [Weaver, Clark] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Weaver, Clark; Herman, Jay; Labow, Gordon; Larko, David; Huang, L. -K.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
[Herman, Jay] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol Ctr, Catonsville, MD USA.
[Labow, Gordon; Larko, David; Huang, L. -K.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Weaver, C (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 614, Greenbelt, MD 20771 USA.
EM clark.j.weaver@nasa.gov
OI Herman, Jay/0000-0002-9146-1632
FU NASA MEaSUREs Project
FX This research is supported by the NASA MEaSUREs Project. We appreciate
helpful discussions with Matthew Deland, Stacey Frith, P. K. Bhartia,
Mathew Zelinka, and Andrew Dessler. We also appreciate the comments of
two anonymous reviewers.
NR 19
TC 0
Z9 0
U1 3
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD DEC
PY 2015
VL 28
IS 23
BP 9473
EP 9488
DI 10.1175/JCLI-D-14-00551.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CX7DC
UT WOS:000365860500025
ER
PT J
AU Gill, SJ
Lowenberg, MH
Neild, SA
Crespo, LG
Krauskopf, B
Puyou, G
AF Gill, Stephen J.
Lowenberg, Mark H.
Neild, Simon A.
Crespo, Luis G.
Krauskopf, Bernd
Puyou, Guilhem
TI Nonlinear Dynamics of Aircraft Controller Characteristics Outside the
Standard Flight Envelope
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID ADAPTIVE CONTROLLER
AB In this paper, the influence of the flight control system over the offnominal behavior of a remotely operated air vehicle is evaluated. Of particular interest is the departure/upset characteristics of the closed-loop system near and beyond stall. The study vehicle is the NASA Generic Transport Model, and both fixed-gain and gain-scheduled versions of a linear quadratic regulator controller with proportional and integral components are evaluated. Bifurcation analysis is used to characterize spiral and spin behavior of the aircraft in closed-loop form and yields an understanding of the underlying vehicle dynamics outside the standard flight envelope. The use of a gain parameter to scale the controller gains provides information on the sensitivity of stability to gain variation, along with tracking how the controller modifies the open-loop steady states. Hence, this provides a means of assessing the effectiveness of the controller and evaluating the upset tendencies of the aircraft.
C1 [Gill, Stephen J.] Univ Bristol, Dept Aerosp Engn, Bristol BS8 1TR, Avon, England.
[Lowenberg, Mark H.] Univ Bristol, Dept Aerosp Engn, Flight Dynam, Bristol BS8 1TR, Avon, England.
[Neild, Simon A.] Univ Bristol, Dept Aerosp Engn, Nonlinear Struct Dynam, Bristol BS8 1TR, Avon, England.
[Crespo, Luis G.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Krauskopf, Bernd] Univ Auckland, Dept Math, Fac Sci, Appl Math, Auckland 1142, New Zealand.
[Puyou, Guilhem] Airbus Ind, Airbus Res & Technology, F-31060 Toulouse 03, France.
RP Gill, SJ (reprint author), Univ Bristol, Dept Aerosp Engn, Bristol BS8 1TR, Avon, England.
RI Lowenberg, Mark/A-5598-2012;
OI Lowenberg, Mark/0000-0002-1373-8237; Krauskopf,
Bernd/0000-0002-8940-230X
FU U.K. Engineering and Physical Sciences Research Council studentship;
Royal Society International Exchanges Scheme [IE121367]
FX The research of Stephen J. Gill was supported by a U.K. Engineering and
Physical Sciences Research Council studentship in collaboration with
Airbus Industries. This work collaboration was supported by the Royal
Society International Exchanges Scheme grant no. IE121367. The authors
are grateful to colleagues at the NASA Langley Research Center Flight
Dynamics Branch and Dynamics Systems and Control Branch for provision of
the Generic Transport Model and advice on its use.
NR 14
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Z9 5
U1 2
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD DEC
PY 2015
VL 38
IS 12
BP 2301
EP 2308
DI 10.2514/1.G000966
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CX5ML
UT WOS:000365745700005
ER
PT J
AU Work, TM
Dagenais, J
Breeden, R
Schneemann, A
Sung, J
Hew, B
Balazs, GH
Berestecky, JM
AF Work, Thierry M.
Dagenais, Julie
Breeden, Renee
Schneemann, Anette
Sung, Joyce
Hew, Brian
Balazs, George H.
Berestecky, John M.
TI Green Turtles (Chelonia mydas) Have Novel Asymmetrical Antibodies
SO JOURNAL OF IMMUNOLOGY
LA English
DT Article
ID STREPTOCOCCAL PROTEIN-G; IMMUNOGLOBULIN GENES; IMMUNE-RESPONSE;
MONOCLONAL-ANTIBODIES; DUCK IMMUNOGLOBULINS; PSAMMOPHIS-SIBILANS;
SEA-TURTLE; EVOLUTION; SYSTEM; PURIFICATION
AB Igs in vertebrates comprise equally sized H and L chains, with exceptions such as H chain-only Abs in camels or natural Ag receptors in sharks. In Reptilia, Igs are known as IgYs. Using immunoassays with isotype-specific mAbs, in this study we show that green turtles (Chelonia mydas) have a 5.7S 120-kDa IgY comprising two equally sized H/L chains with truncated Fc and a 7S 200-kDa IgY comprised of two differently sized H chains bound to L chains and apparently often noncovalently associated with an antigenically related 90-kDa moiety. Both the 200- and 90-kDa 7S molecules are made in response to specific Ag, although the 90-kDa molecule appears more prominent after chronic Ag stimulation. Despite no molecular evidence of a hinge, electron microscopy reveals marked flexibility of Fab arms of 7S and 5.7S IgY. Both IgY can be captured with protein G or melon gel, but less so with protein A. Thus, turtle IgY share some characteristics with mammalian IgG. However, the asymmetrical structure of some turtle Ig and the discovery of an Ig class indicative of chronic antigenic stimulation represent striking advances in our understanding of immunology.
C1 [Work, Thierry M.; Dagenais, Julie; Breeden, Renee] US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, Honolulu, HI 96850 USA.
[Schneemann, Anette; Sung, Joyce] Nanoimaging Serv Inc, San Diego, CA 92121 USA.
[Hew, Brian; Berestecky, John M.] Kapiolani Community Coll, Microbiol Math Sci Dept, Honolulu, HI 96816 USA.
[Balazs, George H.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
RP Work, TM (reprint author), US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, POB 50187, Honolulu, HI 96850 USA.
EM thierry_work@usgs.gov
NR 48
TC 0
Z9 0
U1 2
U2 9
PU AMER ASSOC IMMUNOLOGISTS
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 0022-1767
EI 1550-6606
J9 J IMMUNOL
JI J. Immunol.
PD DEC 1
PY 2015
VL 195
IS 11
BP 5452
EP 5460
DI 10.4049/jimmunol.1501332
PG 9
WC Immunology
SC Immunology
GA CX3NP
UT WOS:000365606100039
PM 26500346
ER
PT J
AU Suhir, E
Ghaffarian, R
AF Suhir, Ephraim
Ghaffarian, Reza
TI Predicted stresses in a ball-grid-array (BGA)/column-grid-array (CGA)
assembly with a low modulus solder at its ends
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID IDENTICAL NONDEFORMABLE ADHERENDS; ADHESIVELY BONDED ASSEMBLIES;
INTERFACIAL THERMAL-STRESSES; BIMETAL THERMOSTATS; BONDING LAYER;
STRAINS; JOINTS; EDGE
AB A simple, easy-to-use and physically meaningful predictive model is suggested for the assessment of thermal stresses in a ball-grid-array or a column-grid-array with a low modulus solder material at the peripheral portions of the assembly. It is shown that the application of such a design can lead to a considerable relief in the interfacial stresses, even to an extent that inelastic strains in the solder joints could be avoided. If this happens, the fatigue strength of the bond and of the assembly as a whole will be improved dramatically: low-cycle fatigue conditions will be replaced by the elastic fatigue condition, and Palmgren-Minor rule of linear accumulation of damages could be used instead of one of the numerous Coffin-Manson models to assess the lifetime of the material.
C1 [Suhir, Ephraim] Portland State Univ, Portland, OR 97207 USA.
[Suhir, Ephraim] Vienna Univ Technol, A-1060 Vienna, Austria.
[Suhir, Ephraim] ERS Co, Los Altos, CA 94024 USA.
[Ghaffarian, Reza] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.
EM suhire@aol.com
NR 65
TC 2
Z9 2
U1 0
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD DEC
PY 2015
VL 26
IS 12
SI SI
BP 9680
EP 9688
DI 10.1007/s10854-015-3635-6
PG 9
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA CX2KP
UT WOS:000365525900053
ER
PT J
AU Suhir, E
Ghaffarian, R
Nicolics, J
AF Suhir, Ephraim
Ghaffarian, Reza
Nicolics, Johann
TI Could application of column-grid-array (CGA) technology result in
inelastic-strain-free state-of-stress in solder material?
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID FATIGUE LIFE PREDICTION; JOINTS; RELIABILITY; PACKAGES; SNAGCU; MODELS
AB Physically meaningful and easy-to-use analytical stress model is developed for a short cylinder (beam) clamped at the ends and subjected to bending caused by the ends offset. The offset is due, in its turn, to an external lateral force that has to be determined from the known offset. It is envisioned that such a beam can adequately represent the state of stress in a column-grid-array (CGA) solder joint interconnection experiencing thermal loading due to the thermal expansion/contraction mismatch of the IC package and the printed circuit board (PCB). The CGA designs are characterized by considerably higher stand-off heights than ball-grid-array (BGA) systems. The offset Delta = l Delta alpha I"t for a CGA solder joint located at the distance l from the mid-cross-section of the package/PCB assembly (the neutral point (DNP)), can be determined, in an approximate analysis, as a product of this distance and the "external" thermal mismatch strain Delta alpha I"t between the IC package and the printed circuit board (PCB). Here Delta alpha is the difference in the effective coefficients of thermal expansion (CTE) of the PCB and package materials, and Delta t is the change in temperature. The objective of the analysis is to demonstrate that the application of a CGA design, in which the solder joints are configured as short clamped-clamped beams, enables one not only to significantly relieve the thermally induced stresses, compared to the BGA system, but possibly to do that to an extent that the stresses in the solder material would remain within the elastic range. If this is achieved, the low-cycle-fatigue condition for the solder material will be replaced by the elastic-fatigue condition, thereby leading to a significantly longer fatigue lifetime of the joint. The elastic fatigue lifetime can be assessed, as is known, based on the Palmgren-Miner rule of linear accumulation of damages. Our analysis is limited therefore to elastic deformations.
C1 [Suhir, Ephraim] Portland State Univ, Portland, OR 97207 USA.
[Suhir, Ephraim] ERS Co, Los Altos, CA 94024 USA.
[Ghaffarian, Reza] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suhir, Ephraim; Nicolics, Johann] Vienna Univ Technol, A-1040 Vienna, Austria.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.
EM suhire@aol.com; reza.ghaffarian@jpl.nasa.gov;
Johann.Nicolics@tuwien.ac.at
NR 30
TC 4
Z9 4
U1 2
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD DEC
PY 2015
VL 26
IS 12
SI SI
BP 10062
EP 10067
DI 10.1007/s10854-015-3688-6
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA CX2KP
UT WOS:000365525900105
ER
PT J
AU Pearson, JC
Daly, AM
Lees, RM
AF Pearson, John C.
Daly, Adam M.
Lees, Ronald M.
TI Unraveling torsional bath interactions with the CO stretching state in
methanol
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Methanol; Infrared; Microwave; Internal rotation; Torsion rotation
vibration interactions
ID MICROWAVE SIDE-BAND; SUB-DOPPLER SPECTROSCOPY; GASEOUS METHYL-ALCOHOL;
DIODE-LASER SPECTRA; 10 MU-M; CO2-LASER LINES; RESONANCE SPECTROSCOPY;
FUNDAMENTAL-BAND; CH3OH; ROTATION
AB Quantum mechanical models describing the effects of a C-3 internal rotor have been successful in modeling all the torsional manifolds of isolated vibrational states. However, modeling the coupling between nearly degenerate small amplitude vibrations in the C-3 internal rotation case remains far from satisfactory and a variety of practical and fundamental questions persist on basis sets, the relative importance of effects and how the problem should be approached. The v(8) C-O stretching state of methanol has been well studied with infrared techniques and has the potential to serve as an experimental reference data set for the development of models for the coupled large and small amplitude motion case. A combined infrared-microwave study of the lowest K A-states of v(t) = 3, v(t) = 4 and v(8) has been performed to understand the nature of the interactions between v(8) the excited torsional states. The interaction between v(t) = 4 and v(8) at K = 0(+) has been confirmed to be Fermi type with magnitude of 2.5 cm(-1). Additionally, the fundamental a-symmetry and b-symmetry Coriolis interactions between v(t) = 3 and v(8) have been estimated to be 8900 MHz and -360 MHz, respectively. The magnitude of these interactions suggests that modeling the v(8) state, the v(t) = 3 state, and the v(t) = 4 states will have to carefully account for these interactions. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Pearson, John C.; Daly, Adam M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lees, Ronald M.] Univ New Brunswick, Dept Phys, St John, NB E2L 4L5, Canada.
RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM John.C.Pearson@jpl.nasa.gov
FU Natural Sciences and Engineering Research Council of Canada; NSERC; NRC;
CIHR; University of Saskatchewan
FX A portion of this research was performed at the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
National Aeronautics and Space Administration. J.C.P. and A.M.D. thank
Peter Groner for numerous useful discussions on the topic of
torsion-rotation-vibration interactions and for comments on early
versions of this manuscript. R.M.L. acknowledges financial support from
the Natural Sciences and Engineering Research Council of Canada. The
Canadian Light Source Inc. is supported by NSERC, NRC, CIHR and the
University of Saskatchewan. We thank Dom Appadoo and Brant Billinghurst
for assistance with the synchrotron FIR spectral measurements at CLS.
NR 44
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U1 2
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD DEC
PY 2015
VL 318
BP 70
EP 77
DI 10.1016/j.jms.2015.08.008
PG 8
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA CX1MC
UT WOS:000365459300009
ER
PT J
AU Weerts, AP
Pattyn, N
Putcha, L
Hoag, SW
Van Ombergen, A
Hallgren, E
Van de Heyning, PH
Wuyts, FL
AF Weerts, Aurelie P.
Pattyn, Nathalie
Putcha, Lakshmi
Hoag, Stephen W.
Van Ombergen, Angelique
Hallgren, Emma
Van de Heyning, Paul H.
Wuyts, Floris L.
TI Restricted sedation and absence of cognitive impairments after
administration of intranasal scopolamine
SO JOURNAL OF PSYCHOPHARMACOLOGY
LA English
DT Article
DE Space motion sickness; intranasal scopolamine; working memory;
short-term memory; implicit memory
ID SPACE MOTION SICKNESS; HEALTHY-YOUNG VOLUNTEERS; WORKING-MEMORY
CAPACITY; SLEEPINESS SCALE; HUMANS; BIOAVAILABILITY; ATTENTION
AB Introduction: Space motion sickness in astronauts during spaceflight causes significant discomfort, which might impede their functionality. Pharmacological treatment has been mainly restricted to promethazine. Transdermal and oral scopolamine have also been used in space; however, their use was reduced due to unpredictable effectiveness and side effects. Recently, intranasal scopolamine administration has gained much interest, since this route ensures fast and reliable absorption with a decreased incidence of undesirable side effects. The aim of this study was to evaluate the effect of intranasal scopolamine on cognitive performance and to determine its side effects.
Methods: This double-blind, placebo controlled, repeated measures study evaluated vigilant attention, short-term memory, implicit memory and working memory. Side effects were reported on a 22-item questionnaire and sleepiness was assessed by the Karolinska, Stanford and Epworth Sleepiness Scales.
Results: Scopolamine had no effect on cognitive function. Only the Karolinska score was significantly increased for scopolamine compared to placebo. Participants reported a dry mouth and dizziness after receiving scopolamine.
Discussion: Results show that intranasal scopolamine did not impair cognitive performance. Intranasal scopolamine might be a good alternative to promethazine for the alleviation of space motion sickness, since the agent has minimal sedative effects and does not hamper cognitive performance.
C1 [Weerts, Aurelie P.; Van Ombergen, Angelique; Hallgren, Emma; Van de Heyning, Paul H.; Wuyts, Floris L.] Univ Antwerp, Univ Antwerp Hosp, Res Ctr Equilibrium & Aerosp AUREA, B-2020 Antwerp, Belgium.
[Weerts, Aurelie P.; Van Ombergen, Angelique; Hallgren, Emma; Van de Heyning, Paul H.; Wuyts, Floris L.] Univ Antwerp, B-2020 Antwerp, Belgium.
[Pattyn, Nathalie] Royal Mil Acad, Dept LIFE, Res Unit VIPER, Brussels, Belgium.
[Pattyn, Nathalie] Vrije Univ Brussel, Dept Expt & Appl Psychol, Res Unit Biol Psychol, Brussels, Belgium.
[Putcha, Lakshmi] NASA, Lyndon B Johnson Space Ctr, Biomed Operat & Res Branch, Houston, TX 77058 USA.
[Hoag, Stephen W.] Univ Maryland, Dept Pharmaceut Sci, Sch Pharm, Baltimore, MD 21201 USA.
RP Wuyts, FL (reprint author), Univ Antwerp, Res Ctr Equilibrium & Aerosp AUREA, Groenenborgerlaan 171, B-2020 Antwerp, Belgium.
EM Floris.Wuyts@uantwerpen.be
FU European Space Agency [AO-2004-093]; Research Foundation Flanders (FWO
Vlaanderen) [11N6414N]
FX The authors disclosed receipt of the following financial support for the
research, authorship, and/or publication of this article: This research
was made possible by the Belgian Science Policy program PRODEX-9 project
SPIN-D in support of the European Space Agency AO-2004-093 corresponding
project. Angelique Van Ombergen is a research fellow for the Research
Foundation Flanders (FWO Vlaanderen; grant 11N6414N).
NR 30
TC 2
Z9 2
U1 1
U2 2
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0269-8811
EI 1461-7285
J9 J PSYCHOPHARMACOL
JI J. Psychopharmacol.
PD DEC
PY 2015
VL 29
IS 12
BP 1231
EP 1235
DI 10.1177/0269881115598414
PG 5
WC Clinical Neurology; Neurosciences; Pharmacology & Pharmacy; Psychiatry
SC Neurosciences & Neurology; Pharmacology & Pharmacy; Psychiatry
GA CX5MC
UT WOS:000365744800002
PM 26268532
ER
PT J
AU Hackney, KJ
Scott, JM
Hanson, AM
English, KL
Downs, ME
Ploutz-Snyder, LL
AF Hackney, Kyle J.
Scott, Jessica M.
Hanson, Andrea M.
English, Kirk L.
Downs, Meghan E.
Ploutz-Snyder, Lori L.
TI THE ASTRONAUT-ATHLETE: OPTIMIZING HUMAN PERFORMANCE IN SPACE
SO JOURNAL OF STRENGTH AND CONDITIONING RESEARCH
LA English
DT Review
DE spaceflight; exercise countermeasures; dietary supplementation;
pharmaceuticals; aging
ID MUSCLE PROTEIN-SYNTHESIS; HUMAN SKELETAL-MUSCLE; ESSENTIAL AMINO-ACIDS;
LONG-DURATION SPACEFLIGHT; NEUROMUSCULAR ACTIVATION PATTERNS; RANDOMIZED
CONTROLLED-TRIAL; LOWER-LIMB SUSPENSION; PROLONGED BED REST;
OLDER-ADULTS; CREATINE SUPPLEMENTATION
AB Hackney, KJ, Scott, JM, Hanson, AM, English, KL, Downs, ME, and Ploutz- Snyder, LL. The astronaut- athlete: optimizing human performance in space. J Strength Cond Res 29( 12): 35313545, 2015- It is well known that long- duration spaceflight results in deconditioning of neuromuscular and cardiovascular systems, leading to a decline in physical fitness. On reloading in gravitational environments, reduced fitness ( e. g., aerobic capacity, muscular strength, and endurance) could impair human performance, mission success, and crew safety. The level of fitness necessary for the performance of routine and off- nominal terrestrial mission tasks remains an unanswered and pressing question for scientists and flight physicians. To mitigate fitness loss during spaceflight, resistance and aerobic exercise are the most effective countermeasure available to astronauts. Currently, 2.5 h center dot d(-1), 6- 7 d center dot wk-1 is allotted in crew schedules for exercise to be performed on highly specialized hardware on the International Space Station ( ISS). Exercise hardware provides up to 273 kg of loading capability for resistance exercise, treadmill speeds between 0.44 and 5.5 m s(-1), and cycle workloads from 0 and 350 W. Compared to ISS missions, future missions beyond low earth orbit will likely be accomplished with less vehicle volume and power allocated for exercise hardware. Concomitant factors, such as diet and age, will also affect the physiologic responses to exercise training ( e. g., anabolic resistance) in the space environment. Research into the potential optimization of exercise countermeasures through use of dietary supplementation, and pharmaceuticals may assist in reducing physiological deconditioning during long- duration spaceflight and have the potential to enhance performance of occupationally related astronaut tasks ( e. g., extravehicular activity, habitat construction, equipment repairs, planetary exploration, and emergency response).
C1 [Hackney, Kyle J.] N Dakota State Univ, Dept Hlth Nutr & Exercise Sci, Fargo, ND 58105 USA.
[Scott, Jessica M.; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Exercise Physiol & Countermeasures Lab, Houston, TX USA.
[Hanson, Andrea M.] NASA, Exercise Physiol & Countermeasures Lab, Houston, TX USA.
[English, Kirk L.] JES Tech, Exercise Physiol & Countermeasures Lab, Houston, TX USA.
[Downs, Meghan E.] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA.
RP Hackney, KJ (reprint author), N Dakota State Univ, Dept Hlth Nutr & Exercise Sci, Fargo, ND 58105 USA.
EM kyle.hackney@ndsu.edu
FU North Dakota NASA Experimental Program to Stimulate Competitive Research
(EPSCoR)
FX The authors would like to thank all members of the Exercise Physiology
and Countermeasures Laboratory at NASA Johnson Space Center for their
efforts in making this publication possible. The authors are especially
grateful to John DeWitt, PhD, from Wyle, Science, Technology and
Engineering Group, and William Amonette, PhD, at the University of
Houston, Clear Lake, for their helpful suggestions that improved the
manuscript. This work was partially funded by North Dakota NASA
Experimental Program to Stimulate Competitive Research (EPSCoR) to K.J.
Hackney. The results of this study do not constitute endorsement of the
product by the authors or the National Strength and Conditioning
Association.
NR 157
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U1 2
U2 13
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1064-8011
EI 1533-4287
J9 J STRENGTH COND RES
JI J. Strength Cond. Res.
PD DEC
PY 2015
VL 29
IS 12
BP 3531
EP 3545
DI 10.1519/JSC.0000000000001191
PG 15
WC Sport Sciences
SC Sport Sciences
GA CX4ZY
UT WOS:000365710900035
PM 26595138
ER
PT J
AU Montemayor, L
Chernow, V
Greer, JR
AF Montemayor, Lauren
Chernow, Victoria
Greer, Julia R.
TI Materials by design: Using architecture in material design to reach new
property spaces
SO MRS BULLETIN
LA English
DT Article
DE cellular (material form); nanostructure; optical properties; structural
ID 3-DIMENSIONAL PHOTONIC CRYSTALS; MICROSCALE TRUSS STRUCTURES; MECHANICAL
METAMATERIALS; STRUCTURAL PERFORMANCE; WAVE-GUIDES; INFRARED
WAVELENGTHS; CERAMIC NANOLATTICES; SIZE DEPENDENCE; DEFORMATION;
FABRICATION
AB Mimicking the resilience offered by hard biomaterials, such as mollusk shells and beaks, has been among the most sought-after engineering pursuits. Technological advances in fabrication methods have provided pathways for using different materials to create architected structural metamaterials with hierarchy and length scales similar to those found in nature. Inspiration from nature has led to the creation of structural metamaterials, or nanolattices, with enhanced mechanical properties caused by hierarchical ordering at various length scales, ranging from angstroms and nanometers for the material microstructure to microns and millimeters for the macroscale architecture. The inherent periodicity and high surface-area-to-volume ratios of nanolattices make them useful for a variety of applications, including photonics, photovoltaics, phononics, and electrochemical systems. This article provides an overview of current three-dimensional architected metamaterials, including their fabrication methods, properties, applications, and limitations.
C1 [Montemayor, Lauren] Jet Prop Lab, Pasadena, CA USA.
[Chernow, Victoria] CALTECH, Pasadena, CA 91125 USA.
[Greer, Julia R.] CALTECH, Pasadena, CA 91125 USA.
RP Montemayor, L (reprint author), Jet Prop Lab, Pasadena, CA USA.
EM lauren.c.montemayor@jpl.nasa.gov; vchernow@caltech.edu;
jrgreer@caltech.edu
NR 88
TC 8
Z9 8
U1 9
U2 56
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0883-7694
EI 1938-1425
J9 MRS BULL
JI MRS Bull.
PD DEC
PY 2015
VL 40
IS 12
BP 1122
EP 1129
DI 10.1557/mrs.2015.263
PG 8
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA CX5LY
UT WOS:000365744400012
ER
PT J
AU Sekii, T
Appourchaux, T
Fleck, B
Turck-Chieze, S
AF Sekii, Takashi
Appourchaux, Thierry
Fleck, Bernhard
Turck-Chieze, Sylvaine
TI Future Mission Concepts for Helioseismology
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun; Helioseismology; Space missions
ID TIME-DISTANCE HELIOSEISMOLOGY; DYNAMICS-OBSERVATORY SDO; MICHELSON
DOPPLER IMAGER; SOLAR OPTICAL TELESCOPE; CONVECTION ZONE; FLOWS BENEATH;
SOHO MISSION; OSCILLATIONS; HINODE; SUN
AB Future space-mission concepts currently discussed in the helioseismology community are reviewed. One popular idea is to observe the Sun from high latitudes, to explore the polar regions as well as to probe the deep interior using stereoscopic techniques, by combining observations from high latitudes with observations from within the ecliptic plane. Another idea is to stay within the ecliptic plane but still aim for stereoscopic helioseismology for deep layers. A new instrument and a novel mission concept for studying the solar core regions are also discussed.
C1 [Sekii, Takashi] NAOJ, Div Solar & Plasma Astrophys, Mitaka, Tokyo 1818588, Japan.
[Appourchaux, Thierry] Univ Paris 11, Inst Astrophys Spatiale, CNRS UMR8617, Orsay, France.
[Fleck, Bernhard] NASA, ESA Sci Operat Dept, GSFC, Greenbelt, MD 20771 USA.
[Turck-Chieze, Sylvaine] CEA DSM IRFU, CE Saclay, F-91191 Gif Sur Yvette, France.
RP Sekii, T (reprint author), NAOJ, Div Solar & Plasma Astrophys, Mitaka, Tokyo 1818588, Japan.
EM sekii@solar.mtk.nao.ac.jp; Thierry.Appourchaux@ias.u-psud.fr;
bfleck@esa.nascom.nasa.gov; Sylvaine.Turck-Chieze@cea.fr
NR 58
TC 0
Z9 0
U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 196
IS 1-4
BP 285
EP 302
DI 10.1007/s11214-015-0142-2
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5PT
UT WOS:000365755100011
ER
PT J
AU Jakosky, BM
Lin, RP
Grebowsky, JM
Luhmann, JG
Mitchell, DF
Beutelschies, G
Priser, T
Acuna, M
Andersson, L
Baird, D
Baker, D
Bartlett, R
Benna, M
Bougher, S
Brain, D
Carson, D
Cauffman, S
Chamberlin, P
Chaufray, JY
Cheatom, O
Clarke, J
Connerney, J
Cravens, T
Curtis, D
Delory, G
Demcak, S
DeWolfe, A
Eparvier, F
Ergun, R
Eriksson, A
Espley, J
Fang, X
Folta, D
Fox, J
Gomez-Rosa, C
Habenicht, S
Halekas, J
Holsclaw, G
Houghton, M
Howard, R
Jarosz, M
Jedrich, N
Johnson, M
Kasprzak, W
Kelley, M
King, T
Lankton, M
Larson, D
Leblanc, F
Lefevre, F
Lillis, R
Mahaffy, P
Mazelle, C
McClintock, W
McFadden, J
Mitchell, D
Montmessin, F
Morrissey, J
Peterson, W
Possel, W
Sauvaud, JA
Schneider, N
Sidney, W
Sparacino, S
Stewart, AIF
Tolson, R
Toublanc, D
Waters, C
Woods, T
Yelle, R
Zurek, R
AF Jakosky, B. M.
Lin, R. P.
Grebowsky, J. M.
Luhmann, J. G.
Mitchell, D. F.
Beutelschies, G.
Priser, T.
Acuna, M.
Andersson, L.
Baird, D.
Baker, D.
Bartlett, R.
Benna, M.
Bougher, S.
Brain, D.
Carson, D.
Cauffman, S.
Chamberlin, P.
Chaufray, J. -Y.
Cheatom, O.
Clarke, J.
Connerney, J.
Cravens, T.
Curtis, D.
Delory, G.
Demcak, S.
DeWolfe, A.
Eparvier, F.
Ergun, R.
Eriksson, A.
Espley, J.
Fang, X.
Folta, D.
Fox, J.
Gomez-Rosa, C.
Habenicht, S.
Halekas, J.
Holsclaw, G.
Houghton, M.
Howard, R.
Jarosz, M.
Jedrich, N.
Johnson, M.
Kasprzak, W.
Kelley, M.
King, T.
Lankton, M.
Larson, D.
Leblanc, F.
Lefevre, F.
Lillis, R.
Mahaffy, P.
Mazelle, C.
McClintock, W.
McFadden, J.
Mitchell, D. L.
Montmessin, F.
Morrissey, J.
Peterson, W.
Possel, W.
Sauvaud, J. -A.
Schneider, N.
Sidney, W.
Sparacino, S.
Stewart, A. I. F.
Tolson, R.
Toublanc, D.
Waters, C.
Woods, T.
Yelle, R.
Zurek, R.
TI The Mars Atmosphere and Volatile Evolution (MAVEN) Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Atmosphere; Solar-wind interactions; MAVEN
ID OXYGEN-ION PRECIPITATION; MARTIAN ATMOSPHERE; SOLAR-WIND;
MAGNETIC-FIELD; CRUSTAL MAGNETIZATION; PLANETARY-ATMOSPHERES; PLASMA
ACCELERATION; VENUS; ABUNDANCE; EXPRESS
AB The MAVEN spacecraft launched in November 2013, arrived at Mars in September 2014, and completed commissioning and began its one-Earth-year primary science mission in November 2014. The orbiter's science objectives are to explore the interactions of the Sun and the solar wind with the Mars magnetosphere and upper atmosphere, to determine the structure of the upper atmosphere and ionosphere and the processes controlling it, to determine the escape rates from the upper atmosphere to space at the present epoch, and to measure properties that allow us to extrapolate these escape rates into the past to determine the total loss of atmospheric gas to space through time. These results will allow us to determine the importance of loss to space in changing the Mars climate and atmosphere through time, thereby providing important boundary conditions on the history of the habitability of Mars. The MAVEN spacecraft contains eight science instruments (with nine sensors) that measure the energy and particle input from the Sun into the Mars upper atmosphere, the response of the upper atmosphere to that input, and the resulting escape of gas to space. In addition, it contains an Electra relay that will allow it to relay commands and data between spacecraft on the surface and Earth.
C1 [Jakosky, B. M.; Andersson, L.; Baker, D.; Brain, D.; DeWolfe, A.; Eparvier, F.; Ergun, R.; Fang, X.; Holsclaw, G.; Kelley, M.; Lankton, M.; McClintock, W.; Peterson, W.; Possel, W.; Schneider, N.; Stewart, A. I. F.; Woods, T.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Lin, R. P.; Luhmann, J. G.; Curtis, D.; Delory, G.; Halekas, J.; Larson, D.; Lillis, R.; McFadden, J.; Mitchell, D. L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Grebowsky, J. M.; Mitchell, D. F.; Acuna, M.; Bartlett, R.; Benna, M.; Carson, D.; Cauffman, S.; Chamberlin, P.; Cheatom, O.; Connerney, J.; Espley, J.; Folta, D.; Gomez-Rosa, C.; Houghton, M.; Howard, R.; Jarosz, M.; Jedrich, N.; Kasprzak, W.; King, T.; Mahaffy, P.; Morrissey, J.; Sparacino, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Beutelschies, G.; Priser, T.; Habenicht, S.; Johnson, M.; Sidney, W.; Waters, C.] Lockheed Martin Corp, Littleton, CO USA.
[Baird, D.] NASA, JSC, Houston, TX USA.
[Bougher, S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Chaufray, J. -Y.] CNRS, LMD, Paris, France.
[Clarke, J.] Boston Univ, Boston, MA 02215 USA.
[Cravens, T.] Univ Kansas, Lawrence, KS 66045 USA.
[Demcak, S.; Zurek, R.] NASA, JPL, Pasadena, CA USA.
[Eriksson, A.] Swedish Inst Space Phys, Uppsala, Sweden.
[Fox, J.] Wright State Univ, Dayton, OH 45435 USA.
[Leblanc, F.; Lefevre, F.; Montmessin, F.] CNRS, LATMOS, Paris, France.
[Mazelle, C.; Sauvaud, J. -A.; Toublanc, D.] IRAP, Toulouse, France.
[Tolson, R.] Natl Inst Aerosp, Hampton, VA USA.
[Yelle, R.] Univ Arizona, Tucson, AZ USA.
RP Jakosky, BM (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM Bruce.Jakosky@lasp.colorado.edu
RI Peterson, WK/A-8706-2009; Chamberlin, Phillip/C-9531-2012; Clarke,
John/C-8644-2013; Benna, Mehdi/F-3489-2012; Lillis, Robert/A-3281-2008;
Fang, Xiaohua/C-2773-2008;
OI Peterson, WK/0000-0002-1513-6096; Chamberlin,
Phillip/0000-0003-4372-7405; Lillis, Robert/0000-0003-0578-517X; Fang,
Xiaohua/0000-0002-6584-2837; Halekas, Jasper/0000-0001-5258-6128;
SCHNEIDER, NICHOLAS/0000-0001-6720-5519
FU NASA; CNES
FX The MAVEN mission would not have been possible without the incredible
dedication, commitment, and experience of the many hundreds of people
(of all job classifications) who have worked on MAVEN. To call out a few
by name would feel like a disservice to those not mentioned. They each
have our incredible gratitude and appreciation for their efforts. In
addition, we benefitted tremendously from the strong support from each
of our partner organizations. Funding for the MAVEN mission was provided
by NASA, with additional funding from CNES.
NR 81
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 3
EP 48
DI 10.1007/s11214-015-0139-x
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700002
ER
PT J
AU Mahaffy, PR
Benna, M
King, T
Harpold, DN
Arvey, R
Barciniak, M
Bendt, M
Carrigan, D
Errigo, T
Holmes, V
Johnson, CS
Kellogg, J
Kimvilakani, P
Lefavor, M
Hengemihle, J
Jaeger, F
Lyness, E
Maurer, J
Melak, A
Noreiga, F
Noriega, M
Patel, K
Prats, B
Raaen, E
Tan, F
Weidner, E
Gundersen, C
Battel, S
Block, BP
Arnett, K
Miller, R
Cooper, C
Edmonson, C
Nolan, JT
AF Mahaffy, Paul R.
Benna, Mehdi
King, Todd
Harpold, Daniel N.
Arvey, Robert
Barciniak, Michael
Bendt, Mirl
Carrigan, Daniel
Errigo, Therese
Holmes, Vincent
Johnson, Christopher S.
Kellogg, James
Kimvilakani, Patrick
Lefavor, Matthew
Hengemihle, Jerome
Jaeger, Ferzan
Lyness, Eric
Maurer, John
Melak, Anthony
Noreiga, Felix
Noriega, Marvin
Patel, Kiran
Prats, Benito
Raaen, Eric
Tan, Florence
Weidner, Edwin
Gundersen, Cynthia
Battel, Steven
Block, Bruce P.
Arnett, Ken
Miller, Ryan
Cooper, Curt
Edmonson, Charles
Nolan, J. Thomas
TI The Neutral Gas and Ion Mass Spectrometer on the Mars Atmosphere and
Volatile Evolution Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Upper atmospheric composition; Mass spectrometry; Atmospheric
escape
ID MARTIAN ATMOSPHERE; NOBLE-GASES; NITROGEN; ESCAPE; ORIGIN; SHERGOTTITES;
EETA-79001; METEORITES; XENON; PROBE
AB The Neutral Gas and Ion Mass Spectrometer (NGIMS) of the Mars Atmosphere and Volatile Evolution Mission (MAVEN) is designed to measure the composition, structure, and variability of the upper atmosphere of Mars. The NGIMS complements two other instrument packages on the MAVEN spacecraft designed to characterize the neutral upper atmosphere and ionosphere of Mars and the solar wind input to this region of the atmosphere. The combined measurement set is designed to quantify atmosphere escape rates and provide input to models of the evolution of the martian atmosphere. The NGIMS is designed to measure both surface reactive and inert neutral species and ambient ions along the spacecraft track over the 125-500 km altitude region utilizing a dual ion source and a quadrupole analyzer.
C1 [Mahaffy, Paul R.; Benna, Mehdi; King, Todd; Harpold, Daniel N.; Arvey, Robert; Barciniak, Michael; Bendt, Mirl; Carrigan, Daniel; Errigo, Therese; Holmes, Vincent; Johnson, Christopher S.; Kellogg, James; Kimvilakani, Patrick; Lefavor, Matthew; Hengemihle, Jerome; Jaeger, Ferzan; Lyness, Eric; Maurer, John; Melak, Anthony; Noreiga, Felix; Noriega, Marvin; Patel, Kiran; Prats, Benito; Raaen, Eric; Tan, Florence; Weidner, Edwin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gundersen, Cynthia] AMU Engn, Miami, FL 33156 USA.
[Battel, Steven] Battel Engn, Scottsdale, AZ 85253 USA.
[Block, Bruce P.; Arnett, Ken; Miller, Ryan; Cooper, Curt; Edmonson, Charles] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Nolan, J. Thomas] Nolan Engn, Kensington, MD 20895 USA.
RP Mahaffy, PR (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Paul.R.Mahaffy@nasa.gov
RI Benna, Mehdi/F-3489-2012
FU Science Mission Directorate of the National Aeronautics and Space
Administration
FX The NGIMS development was funded by the Science Mission Directorate of
the National Aeronautics and Space Administration.
NR 44
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 49
EP 73
DI 10.1007/s11214-014-0091-1
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700003
ER
PT J
AU Connerney, JEP
Espley, J
Lawton, P
Murphy, S
Odom, J
Oliversen, R
Sheppard, D
AF Connerney, J. E. P.
Espley, J.
Lawton, P.
Murphy, S.
Odom, J.
Oliversen, R.
Sheppard, D.
TI The MAVEN Magnetic Field Investigation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Magnetic field; Magnetometer; MAVEN; Spaceflight instrumentation;
Spacecraft magnetic control; Magnetic cleanliness
ID MARS CRUSTAL MAGNETISM; SOLAR-WIND INTERACTION; EARLY PLATE-TECTONICS;
THERMAL EVOLUTION; HISTORY; MAGNETOSPHERES; MAGNETOMETERS; ATMOSPHERE;
AURORA
AB The MAVEN magnetic field investigation is part of a comprehensive particles and fields subsystem that will measure the magnetic and electric fields and plasma environment of Mars and its interaction with the solar wind. The magnetic field instrumentation consists of two independent tri-axial fluxgate magnetometer sensors, remotely mounted at the outer extremity of the two solar arrays on small extensions ("boomlets"). The sensors are controlled by independent and functionally identical electronics assemblies that are integrated within the particles and fields subsystem and draw their power from redundant power supplies within that system. Each magnetometer measures the ambient vector magnetic field over a wide dynamic range (to 65,536 nT per axis) with a resolution of 0.008 nT in the most sensitive dynamic range and an accuracy of better than 0.05 %. Both magnetometers sample the ambient magnetic field at an intrinsic sample rate of 32 vector samples per second. Telemetry is transferred from each magnetometer to the particles and fields package once per second and subsequently passed to the spacecraft after some reformatting. The magnetic field data volume may be reduced by averaging and decimation, when necessary to meet telemetry allocations, and application of data compression, utilizing a lossless 8-bit differencing scheme. The MAVEN magnetic field experiment may be reconfigured in flight to meet unanticipated needs and is fully hardware redundant. A spacecraft magnetic control program was implemented to provide a magnetically clean environment for the magnetic sensors and the MAVEN mission plan provides for occasional spacecraft maneuvers-multiple rotations about the spacecraft and axes-to characterize spacecraft fields and/or instrument offsets in flight.
C1 [Connerney, J. E. P.; Espley, J.; Odom, J.; Oliversen, R.; Sheppard, D.] NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Lawton, P.] ADNET Syst Inc, Bethesda, MD USA.
[Murphy, S.] Rocket Sci Inc, West Friendship, MD USA.
RP Connerney, JEP (reprint author), NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM jack.connerney@nasa.gov
OI connerney, jack/0000-0001-7478-6462
NR 49
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U2 17
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 257
EP 291
DI 10.1007/s11214-015-0169-4
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700009
ER
PT J
AU Eparvier, FG
Chamberlin, PC
Woods, TN
Thiemann, EMB
AF Eparvier, F. G.
Chamberlin, P. C.
Woods, T. N.
Thiemann, E. M. B.
TI The Solar Extreme Ultraviolet Monitor for MAVEN
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Solar irradiance; Extreme ultraviolet; Mars; MAVEN
AB The Extreme Ultraviolet (EUV) monitor is an instrument on the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission, designed to measure the variability of the solar soft x-rays and EUV irradiance at Mars. The solar output in this wavelength range is a primary energy input to the Mars atmosphere and a driver for the processes leading to atmospheric escape. The MAVEN EUV monitor consists of three broadband radiometers. The radiometers consist of silicon photodiodes with different bandpass-limiting filters for each channel. The filters for the radiometers are: Channel A: thin foil C/Al/Nb/C for 0.1-3 nm and 17-22 nm, Channel B: thin foil C/Al/Ti/C for 0.1-7 nm, and Channel C: interference filter for 121-122 nm. A fourth, covered photodiode is used to monitor variations in dark signal due to temperature and radiation background changes. The three science channels will monitor emissions from the highly variable corona and transition region of the solar atmosphere. The EUV monitor is mounted on the top deck of the MAVEN spacecraft and is pointed at the Sun for most of its orbit around Mars. The measurement cadence is 1-second. The broadband irradiances can be used to monitor the most rapid changes in solar irradiance due to flares. In combination with time-interpolated observations at Earth of slower varying solar spectral emissions, the broadband MAVEN EUV monitor measurements will also be used in a spectral irradiance model to generate the full EUV spectrum at Mars from 0 to 190 nm in 1-nm bins on a time cadence of 1-minute and daily averages.
C1 [Eparvier, F. G.; Woods, T. N.; Thiemann, E. M. B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Chamberlin, P. C.] NASA, Goddard Spaceflight Ctr, Greenbelt, MD USA.
RP Eparvier, FG (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM eparvier@colorado.edu; phillip.c.chamberlin@nasa.gov;
tom.woods@lasp.colorado.edu; ed.thiemann@lasp.colorado.edu
RI Chamberlin, Phillip/C-9531-2012;
OI Chamberlin, Phillip/0000-0003-4372-7405; EPARVIER,
FRANCIS/0000-0001-7143-2730
FU NASA MAVEN [NNH10CC04C]
FX The authors are grateful to the large number of people who have
contributed to the success of this project. In particular we want to
acknowledge all the engineers working on the EUV instrument and the
Particles and Fields Package. The work was made under NASA MAVEN
contract (NNH10CC04C).
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 293
EP 301
DI 10.1007/s11214-015-0195-2
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700010
ER
PT J
AU Zurek, RW
Tolson, RH
Baird, D
Johnson, MZ
Bougher, SW
AF Zurek, Richard W.
Tolson, Robert H.
Baird, Darren
Johnson, Mark Z.
Bougher, Stephen W.
TI Application of MAVEN Accelerometer and Attitude Control Data to Mars
Atmospheric Characterization
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE MAVEN; Mars; Atmosphere; Density and temperature characterization
ID AEROBRAKING OPERATIONS; GLOBAL SURVEYOR; THERMOSPHERE
AB The structure of the upper atmosphere of Mars (above similar to 100 km) has been probed in situ mainly using spacecraft accelerometers during the aerobraking phases of 3 Mars orbiters. In a similar manner, the Mars Atmosphere and Volatile Evolution (MAVEN) Accelerometer Experiment (ACC) will also use atmospheric drag accelerations sensed by inertial measurement units (IMU) onboard the spacecraft to recover atmospheric density along the orbiter path. These densities are used to estimate hydrostatic 'vertical' density and temperature profiles, along track and altitudinal density waves, and latitudinal and longitudinal density variations. The IMU accelerometer signal-to-noise should permit profile reconstructions from spacecraft periapsis, nominally at 150 km altitude, to similar to 170 km, an altitude range nominally spanning densities of 0.05-0.15 kg/km(3). However, in situ measurements over a much greater altitude range, down to similar to 125 km (reaching densities of similar to 2-3.5 kg/km(3)), can be made during each of five week-long "Deep Dip" (DD) campaigns, and these are the prime focus of the Accelerometer Experiment. Judicious choice of the timing of these Deep-Dip campaigns during the MAVEN periapsis progression through local time, latitude and longitude in both hemispheres and in different seasons will add significantly to the existing data base of lower thermospheric densities. Other IMU and attitude control data may be used to estimate torques in order to improve the atmospheric density analysis, especially in the higher altitudes of the nominal science orbit, and, more challengingly, to estimate cross-track winds during the Deep-Dips.
C1 [Zurek, Richard W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tolson, Robert H.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Baird, Darren] NASA, Johnson Space Flight Ctr, Houston, TX 77058 USA.
[Johnson, Mark Z.] Lockheed Martin Space Syst Corp, Denver, CO USA.
[Bougher, Stephen W.] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Zurek, RW (reprint author), CALTECH, Jet Prop Lab, Mail Stop 321-690,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM richard.w.zurek@jpl.nasa.gov
FU NASA; Jet Propulsion Laboratory, California Institute of Technology
FX This work was sponsored by NASA, including a part under contract through
the Jet Propulsion Laboratory, California Institute of Technology.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 303
EP 317
DI 10.1007/s11214-014-0095-x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700011
ER
PT J
AU Grebowsky, J
Fast, K
Talaat, E
Combi, M
Crary, F
England, S
Ma, Y
Mendillo, M
Rosenblatt, P
Seki, K
Stevens, M
Withers, P
AF Grebowsky, J.
Fast, K.
Talaat, E.
Combi, M.
Crary, F.
England, S.
Ma, Y.
Mendillo, M.
Rosenblatt, P.
Seki, K.
Stevens, M.
Withers, P.
TI Science Enhancements by the MAVEN Participating Scientists
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Aeronomy; Thermosphere; Ionosphere magnetosphere MAVEN mission
ID KELVIN-HELMHOLTZ INSTABILITY; CO2 ICE CLOUDS; UPPER-ATMOSPHERE;
MAGNETIC-FIELD; SOLAR-WIND; MARTIAN IONOSPHERE; HYBRID SIMULATION; RADAR
SOUNDINGS; MARS EXPRESS; PICKUP IONS
AB NASA implemented a Participating Scientist Program and released a solicitation for the Mars Atmosphere and Volatile EvolutioN mission (MAVEN) proposals on February 14, 2013. After a NASA peer review panel evaluated the proposals, NASA Headquarters selected nine on June 12, 2013. The program's intent is to enhance the science return from the mission by including new investigations that broaden and/or complement the baseline investigations, while still addressing key science goals. The selections cover a broad range of science investigations. Included are: a patching of a 3D exosphere model to an improved global ionosphere-thermosphere model to study the generation of the exosphere and calculate the escape rates; the addition of a focused study of upper atmosphere variability and waves; improvement of a multi-fluid magnetohydrodynamic model that will be adjusted according to MAVEN observations to enhance the understanding of the solar-wind plasma interaction; a global study of the state of the ionosphere; folding MAVEN measurements into the Mars International Reference Ionosphere under development; quantification of atmospheric loss by pick-up using ion cyclotron wave observations; the reconciliation of remote and in situ observations of the upper atmosphere; the application of precise orbit determination of the spacecraft to measure upper atmospheric density and in conjunction with other Mars missions improve the static gravity field model of Mars; and an integrated ion/neutral study of ionospheric flows and resultant heavy ion escape. Descriptions of each of these investigations are given showing how each adds to and fits seamlessly into MAVEN mission science design.
C1 [Grebowsky, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fast, K.; Talaat, E.] NASA, Headquarters, Washington, DC 20546 USA.
[Combi, M.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Crary, F.] Univ Colorado, Boulder, CO 80303 USA.
[England, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ma, Y.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Mendillo, M.; Withers, P.] Boston Univ, Boston, MA 02215 USA.
[Rosenblatt, P.] Royal Observ Belgium, Brussels, Belgium.
[Seki, K.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Stevens, M.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Grebowsky, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joseph.m.grebowsky@nasa.gov
RI Combi, Michael/J-1697-2012; Ma, Yingjuan/B-4895-2017
OI Combi, Michael/0000-0002-9805-0078; Ma, Yingjuan/0000-0003-2584-7091
FU NASA's MAVEN Participating Scientist Program
FX Support from NASA's MAVEN Participating Scientist Program is
acknowledged for all the studies.
NR 105
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 319
EP 355
DI 10.1007/s11214-014-0080-4
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700012
ER
PT J
AU Lillis, RJ
Brain, DA
Bougher, SW
Leblanc, F
Luhmann, JG
Jakosky, BM
Modolo, R
Fox, J
Deighan, J
Fang, X
Wang, YC
Lee, Y
Dong, C
Ma, Y
Cravens, T
Andersson, L
Curry, SM
Schneider, N
Combi, M
Stewart, I
Clarke, J
Grebowsky, J
Mitchell, DL
Yelle, R
Nagy, AF
Baker, D
Lin, RP
AF Lillis, R. J.
Brain, D. A.
Bougher, S. W.
Leblanc, F.
Luhmann, J. G.
Jakosky, B. M.
Modolo, R.
Fox, J.
Deighan, J.
Fang, X.
Wang, Y. C.
Lee, Y.
Dong, C.
Ma, Y.
Cravens, T.
Andersson, L.
Curry, S. M.
Schneider, N.
Combi, M.
Stewart, I.
Clarke, J.
Grebowsky, J.
Mitchell, D. L.
Yelle, R.
Nagy, A. F.
Baker, D.
Lin, R. P.
TI Characterizing Atmospheric Escape from Mars Today and Through Time, with
MAVEN
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Atmosphere; Escape; Maven; Models
ID SOLAR-WIND CONDITIONS; GENERAL-CIRCULATION MODEL; OXYGEN-ION
PRECIPITATION; MARTIAN ATMOSPHERE; PLASMA ENVIRONMENT; MAGNETIZED MARS;
CHARGE-EXCHANGE; SPACE RADIATION; HYDROGEN CORONA; IMPACT EROSION
AB Two of the primary goals of the MAVEN mission are to determine how the rate of escape of Martian atmospheric gas to space at the current epoch depends upon solar influences and planetary parameters and to estimate the total mass of atmosphere lost to space over the history of the planet. Along with MAVEN's suite of nine science instruments, a collection of complementary models of the neutral and plasma environments of Mars' upper atmosphere and near-space environment are an indispensable part of the MAVEN toolkit, for three primary reasons. First, escaping neutrals will not be directly measured by MAVEN and so neutral escape rates must be derived, via models, from in situ measurements of plasma temperatures and neutral and plasma densities and by remote measurements of the extended exosphere. Second, although escaping ions will be directly measured, all MAVEN measurements are limited in spatial coverage, so global models are needed for intelligent interpolation over spherical surfaces to calculate global escape rates. Third, MAVEN measurements will lead to multidimensional parameterizations of global escape rates for a range of solar and planetary parameters, but further global models informed by MAVEN data will be required to extend these parameterizations to the more extreme conditions that likely prevailed in the early solar system, which is essential for determining total integrated atmospheric loss. We describe these modeling tools and the strategies for using them in concert with MAVEN measurements to greater constrain the history of atmospheric loss on Mars.
C1 [Lillis, R. J.; Luhmann, J. G.; Wang, Y. C.; Curry, S. M.; Mitchell, D. L.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brain, D. A.; Jakosky, B. M.; Deighan, J.; Fang, X.; Dong, C.; Andersson, L.; Schneider, N.; Stewart, I.; Baker, D.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Bougher, S. W.; Lee, Y.; Combi, M.; Nagy, A. F.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Leblanc, F.; Modolo, R.] Meteorol Dynam Lab, Paris, France.
[Fox, J.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA.
[Ma, Y.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Cravens, T.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Clarke, J.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Grebowsky, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yelle, R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM rlillis@SSL.Berkeley.edu
RI Dong, Chuanfei/E-6485-2010; Combi, Michael/J-1697-2012; Clarke,
John/C-8644-2013; Lillis, Robert/A-3281-2008; Fang, Xiaohua/C-2773-2008;
Ma, Yingjuan/B-4895-2017;
OI Dong, Chuanfei/0000-0002-8990-094X; Combi, Michael/0000-0002-9805-0078;
Lillis, Robert/0000-0003-0578-517X; Fang, Xiaohua/0000-0002-6584-2837;
Ma, Yingjuan/0000-0003-2584-7091; SCHNEIDER,
NICHOLAS/0000-0001-6720-5519
NR 172
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U1 2
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 357
EP 422
DI 10.1007/s11214-015-0165-8
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700013
ER
PT J
AU Bougher, SW
Cravens, TE
Grebowsky, J
Luhmann, J
AF Bougher, S. W.
Cravens, T. E.
Grebowsky, J.
Luhmann, J.
TI The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere
Reservoir That Regulates Volatile Escape
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mars; Aeronomy; Thermosphere; Ionosphere; MAVEN Mission
ID ULTRAVIOLET SPECTROMETER EXPERIMENT; RADIO OCCULTATION MEASUREMENTS;
GLOBAL SURVEYOR ACCELEROMETER; MARTIAN UPPER-ATMOSPHERE; SOLAR-CYCLE
VARIATION; HOT OXYGEN-ATOMS; AEROBRAKING OPERATIONS; MAGNETIC-FIELD;
THERMAL TIDES; INTERANNUAL VARIABILITY
AB The Mars thermosphere-ionosphere-exosphere (TIE) system constitutes the atmospheric reservoir (i.e. available cold and hot planetary neutral and thermal ion species) that regulates present day escape processes from the planet. The characterization of this TIE system, including its spatial and temporal (e.g., solar cycle, seasonal, diurnal, episodic) variability is needed to determine present day escape rates. Without knowledge of the physics and chemistry creating this TIE region and driving its variations, it is not possible to constrain either the short term or long term histories of atmosphere escape from Mars. MAVEN (Mars Atmosphere and Volatile Evolution Mission) will make both in-situ and remote measurements of the state variables of the Martian TIE system. A full characterization of the thermosphere (similar to 100-250 km) and ionosphere (similar to 100-400 km) structure (and its variability) will be conducted with the collection of spacecraft in-situ measurements that systematically span most local times and latitudes, over a regular sampling of Mars seasons, and throughout the bottom half of the solar cycle. Such sampling will far surpass that available from existing spacecraft and ground-based datasets. In addition, remote measurements will provide a systematic mapping of the composition and structure of Mars neutral upper atmosphere and coronae (e.g. H, C, N, O), as well as probe lower altitudes. Such a detailed characterization is a necessary first step toward answering MAVEN's three main science questions (see Jakosky et al. 2014, this issue). This information will be used to determine present day escape rates from Mars, and provide an estimate of integrated loss to space throughout Mars history.
C1 [Bougher, S. W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Grebowsky, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Luhmann, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Bougher, SW (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM bougher@umich.edu
NR 143
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U1 5
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2015
VL 195
IS 1-4
BP 423
EP 456
DI 10.1007/s11214-014-0053-7
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CX5GI
UT WOS:000365729700014
ER
PT J
AU Mazanek, DD
Merrill, RG
Brophy, JR
Mueller, RP
AF Mazanek, Daniel D.
Merrill, Raymond G.
Brophy, John R.
Mueller, Robert P.
TI Asteroid Redirect Mission concept: A bold approach for utilizing space
resources
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 65th International Astronautical Congress (IAC)
CY SEP 29-OCT 03, 2014
CL Toronto, CANADA
SP Canadian Aeronaut & Space Inst, Int Astronaut Assoc
DE Asteroid resources; In-situ resource utilization (ISRU); Solar electric
propulsion; Asteroid Redirect Mission; Space exploration; Settlement of
space
ID CERES
AB The utilization of natural resources from asteroids is an idea that is older than the Space Age. The technologies are now available to transform this endeavor from an idea into reality. The Asteroid Redirect Mission (ARM) is a mission concept which includes the goal of robotically returning a small Near-Earth Asteroid (NEA) or a multi-ton boulder from a large NEA to cislunar space in the mid-2020s using an advanced Solar Electric Propulsion (SEP) vehicle and currently available technologies. The paradigm shift enabled by the ARM concept would allow in-situ resource utilization (ISRU) to be used at the human mission departure location (i.e., cislunar space) versus exclusively at the deep-space mission destination. This approach drastically reduces the barriers associated with utilizing ISRU for human deep-space missions. The successful testing of ISRU techniques and associated equipment could enable large-scale commercial ISRU operations to become a reality and enable a future space-based economy utilizing processed asteroidal materials. This paper provides an overview of the ARM concept and discusses the mission objectives, key technologies, and capabilities associated with the mission, as well as how the ARM and associated operations would benefit humanity's quest for the exploration and settlement of space. (C) 2015 Published by Elsevier Ltd. on behalf of IAA.
C1 [Mazanek, Daniel D.; Merrill, Raymond G.; Mueller, Robert P.] NASA, Washington, DC 20456 USA.
[Brophy, John R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Mazanek, DD (reprint author), NASA, Washington, DC 20456 USA.
EM Daniel.D.Mazanek@nasa.gov; Raymond.G.Merrill@nasa.gov;
John.R.Brophy@nasa.gov; Robert.P.Mueller@nasa.gov
NR 15
TC 2
Z9 2
U1 2
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD DEC
PY 2015
VL 117
BP 163
EP 171
DI 10.1016/j.actaastro.2015.06.018
PG 9
WC Engineering, Aerospace
SC Engineering
GA CW2BZ
UT WOS:000364797400015
ER
PT J
AU Cervini-Silva, J
Antonio-Nieto-Camacho
Kaufhold, S
Ufer, K
de Jesus, ER
AF Cervini-Silva, Javiera
Antonio-Nieto-Camacho
Kaufhold, Stephan
Ufer, Kristian
Ronquillo de Jesus, Elba
TI The anti-inflammatory activity of bentonites
SO APPLIED CLAY SCIENCE
LA English
DT Article
DE Edema inhibition; Smectites
ID IN-VITRO BIOCOMPATIBILITY; WATER; ANTIBACTERIAL; ALLOPHANE; CLAYS;
QUANTIFICATION; SUSPENSIONS; CAPACITY; ECUADOR; CEC
AB Bentonites, naturally occurring clays, are produced industrially because of their adsorbent capacity but little is known about their effects on human health. This manuscript reports on the anti-inflammatory activity of bentonites. Bentonites collected from India (Bent-India), Hungary (Bent-Hungary), Argentina (Bent-Argentina), and Indonesia (Bent-Indonesia) were studied. All four bentonites were tested for anti-inflammatory activity using the mouse ear edema and the 12-O-tetradecanoylphorbol-13-acetate (TPA) method. Bentonites inhibited edema after 4 h (El %), regardless of composition. A direct comparison between El and surface area values showed that Bent-Argentina was four times more active than the other bentonites, with infiltration-preferred in the former case. We attributed the inhibition of edema by bentonites to clay swelling, causing physical occlusion thereby limiting the movement of leukocyte cells towards the inflammation site. Expandability over changes in mineral composition underpinned inhibition of edema by bentonites, while evidence lacked to support chemical-transfer mechanism(s). (C) 2015 Elsevier B.V. All rights reserved.
C1 [Cervini-Silva, Javiera; Ronquillo de Jesus, Elba] Univ Autonoma Metropolitana, Dept Proc & Tecnol, Mexico City 05348, DF, Mexico.
[Cervini-Silva, Javiera] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
[Cervini-Silva, Javiera] NASA, Astrobiol Inst, Washington, DC USA.
[Antonio-Nieto-Camacho] Univ Nacl Utonoma Mexico, Inst Quim, Lab Pruebas Biol, Mexico City, DF, Mexico.
[Kaufhold, Stephan; Ufer, Kristian] BGR Bundesansalt Geowissensch & Rohstoffe, D-30655 Hannover, Germany.
RP Cervini-Silva, J (reprint author), Univ Autonoma Metropolitana, Dept Proc & Tecnol, Unidad Cuajimalpa, Av Vasco de Quiroga 4871, Mexico City 05348, DF, Mexico.
EM jcervini@correo.cua.uam.mx
FU Universidad Autonoma Metropolitana Unidad Cuajimalpa [33678]
FX The authors thank Jaime Ortega (UAM-Cuajimalpa) and Natascha Schleuning
(Bundesansaltfur Geowissenschaften und Rohstoffe, BGR) for technical
assistance. This project was supported in part by Universidad Autonoma
Metropolitana Unidad Cuajimalpa (Grant No. 33678).
NR 33
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U1 6
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-1317
EI 1872-9053
J9 APPL CLAY SCI
JI Appl. Clay Sci.
PD DEC
PY 2015
VL 118
BP 56
EP 60
DI 10.1016/j.clay.2015.08.039
PG 5
WC Chemistry, Physical; Materials Science, Multidisciplinary; Mineralogy
SC Chemistry; Materials Science; Mineralogy
GA CW5SH
UT WOS:000365056400007
ER
PT J
AU Ade, PAR
Aikin, RW
Barkats, D
Benton, SJ
Bischoff, CA
Bock, JJ
Brevik, JA
Buder, I
Bullock, E
Dowell, CD
Duband, L
Filippini, JP
Fliescher, S
Golwala, SR
Halpern, M
Hasselfield, M
Hildebrandt, SR
Hilton, GC
Irwin, KD
Karkare, KS
Kaufman, JP
Keating, BG
Kernasovskiy, SA
Kovac, JM
Kuo, CL
Leitch, EM
Lueker, M
Netterfield, CB
Nguyen, HT
O'Brient, R
Ogburn, RW
Orlando, A
Pryke, C
Richter, S
Schwarz, R
Sheehy, CD
Staniszewski, ZK
Sudiwala, RV
Teply, GP
Tolan, JE
Turner, AD
Vieregg, AG
Wong, CL
Yoon, KW
AF Ade, P. A. R.
Aikin, R. W.
Barkats, D.
Benton, S. J.
Bischoff, C. A.
Bock, J. J.
Brevik, J. A.
Buder, I.
Bullock, E.
Dowell, C. D.
Duband, L.
Filippini, J. P.
Fliescher, S.
Golwala, S. R.
Halpern, M.
Hasselfield, M.
Hildebrandt, S. R.
Hilton, G. C.
Irwin, K. D.
Karkare, K. S.
Kaufman, J. P.
Keating, B. G.
Kernasovskiy, S. A.
Kovac, J. M.
Kuo, C. L.
Leitch, E. M.
Lueker, M.
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.
Sudiwala, R. V.
Teply, G. P.
Tolan, J. E.
Turner, A. D.
Vieregg, A. G.
Wong, C. L.
Yoon, K. W.
CA BICEP2 Collaboration
TI BICEP2. III. INSTRUMENTAL SYSTEMATICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; instrumentation: polarimeters; methods: data analysis
ID BACKGROUND POLARIZATION MEASUREMENTS; SPT-SZ SURVEY; POWER SPECTRUM;
GRAVITY-WAVES; MICROWAVE; ANISOTROPY; TELESCOPE; RADIATION; PROBE;
CONSTRAINTS
AB In a companion paper, we have reported a >5 sigma detection of degree scale B-mode polarization at 150 GHz by the BICEP2 experiment. Here we provide a detailed study of potential instrumental systematic contamination to that measurement. We focus extensively on spurious polarization that can potentially arise from beam imperfections. We present a heuristic classification of beam imperfections according to their symmetries and uniformities, and discuss how resulting contamination adds or cancels in maps that combine observations made at multiple orientations of the telescope about its boresight axis. We introduce a technique, which we call "deprojection," for filtering the leading order beam-induced contamination from time-ordered data, and show that it reduces power in BICEP2's actual and null-test BB spectra consistent with predictions using high signal-to-noise beam shape measurements. We detail the simulation pipeline that we use to directly simulate instrumental systematics and the calibration data used as input to that pipeline. Finally, we present the constraints on BB contamination from individual sources of potential systematics. We find that systematics contribute BB power that is a factor of similar to 10x below BICEP2's three-year statistical uncertainty, and negligible compared to the observed BB signal. The contribution to the best-fit tensor/scalar ratio is at a level equivalent to r = (3-6) x 10(-3).
C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aikin, R. W.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Duband, L.] CEA Grenoble, SBT, F-38054 Grenoble, France.
[Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61820 USA.
[Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada.
[Hilton, G. C.; Irwin, K. D.] NIST, Boulder, CO 80305 USA.
[Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Leitch, E. M.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
OI Orlando, Angiola/0000-0001-8004-5054; Karkare,
Kirit/0000-0002-5215-6993; Bischoff, Colin/0000-0001-9185-6514; Barkats,
Denis/0000-0002-8971-1954
FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592,
ANT-1110087]; JPL Research and Technology Development Fund; NASA APRA
program [06-ARPA206-0040, 10-SAT10-0017]; SAT program; Gordon and Betty
Moore Foundation at Caltech; Canada Foundation for Innovation grant; W.
M. Keck Foundation; Kavli Institute for Cosmological Physics at the
University of Chicago [NSF PHY-1125897]; Irene Coyle and Kathy Deniston
FX BICEP2 was supported by the U.S. National Science Foundation under
grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and
ANT-1110087 (Chicago/Minnesota). The development of antenna-coupled
detector technology was supported by the JPL Research and Technology
Development Fund and grants 06-ARPA206-0040 and 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 receiver development was supported in part by a grant
from the W. M. Keck Foundation. Partial support for C. Sheehy was also
provided by the Kavli Institute for Cosmological Physics at the
University of Chicago through grant NSF PHY-1125897 and an endowment
from the Kavli Foundation and its founder Fred Kavli. The computations
in this paper were run on the Odyssey cluster supported by the FAS
Science Division Research Computing Group at Harvard University.
Tireless administrative support was provided by Irene Coyle and Kathy
Deniston.
NR 57
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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 DEC 1
PY 2015
VL 814
IS 2
AR 110
DI 10.1088/0004-637X/814/2/110
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300028
ER
PT J
AU Banerjee, DPK
Nuth, JA
Misselt, KA
Varricatt, WP
Sand, D
Ashok, NM
Su, KYL
Marion, GH
Marengo, M
AF Banerjee, Dipankar. P. K.
Nuth, Joseph A., III
Misselt, Karl A.
Varricatt, Watson P.
Sand, David
Ashok, N. M.
Su, K. Y. L.
Marion, G. H.
Marengo, Massimo
TI EVOLUTION OF THE DUST IN V4332 SAGITTARII
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: stars; novae, cataclysmic variables; stars:
individual (V4332 Sagittarii)
ID MU-M FEATURE; GIANT BRANCH STARS; INFRARED-SPECTRA; CIRCUMSTELLAR DUST;
OPTICAL-PROPERTIES; V838 MONOCEROTIS; SILICATE GRAINS; VAPOR-PRESSURE;
V4332-SAGITTARII; CONDENSATION
AB An eruptive nova-like event took place in 1994 in the stellar-merger candidate V4332 Sgr. Following the eruption, dust consisting of refractory silicate-rich dust grains containing a significant component of AlO bonding was formed sometime between 1998 and 2003. Observations using Spitzer between 2005 and 2009 show significant changes in the 10 mu m silicate stretch feature. There is a deepening of the 10 mu m silicate stretch as well as the development of a feature between about 13 and 20 mu m consistent with a blend of the MgO and FeO stretching features and the O-Si-O bending mode of increasingly ordered silicate dust. Near-infrared observations show the presence of AlO and water vapor in the outflow in 2003, 2004, and 2005: the AlO has significantly decreased in spectra obtained in 2014 while the water vapor remains largely unchanged. An attempt is made to correlate these observations and understand the significance of these changes using DUSTY modeling. The observations appear consistent with the kinetically controlled condensation of highly underoxidized SiO/AlO/Fe/Mg dust grains in the outflow followed by the continuous evolution of the initial condensate due to thermal annealing and oxidation of the dust via reaction with ambient O, OH, and H2O in the expanding, cooling shell. Periodic monitoring of this dust shell over the mid-infrared spectral range could yield useful information on the evolution of underoxidized silicate condensates exposed to hot water vapor in more conventional circumstellar environments.
C1 [Banerjee, Dipankar. P. K.; Ashok, N. M.] Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India.
[Nuth, Joseph A., III] NASA, GSFC, Greenbelt, MD 20771 USA.
[Misselt, Karl A.; Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Varricatt, Watson P.] United Kingdom Infrared Telescope, Hilo, HI 96720 USA.
[Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA.
[Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
RP Banerjee, DPK (reprint author), Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India.
OI Su, Kate/0000-0002-3532-5580; Sand, David/0000-0003-4102-380X
FU Department of Space, Government of India; National Aeronautics and Space
Administration [NNH14CK55B]
FX Research at the Physical Research Laboratory is supported by the
Department of Space, Government of India. D.S. is a Visiting Astronomer
at the Infrared Telescope Facility, which is operated by the University
of Hawaii under contract NNH14CK55B with the National Aeronautics and
Space Administration. He would like to thank Michael Cushing for his
efforts in keeping the Spextool reduction code up to date. We are
grateful to an anonymous referee for helpful comments that improved the
paper and deeply appreciative for the critical, yet favorable,
evaluation of this work.
NR 48
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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 DEC 1
PY 2015
VL 814
IS 2
AR 109
DI 10.1088/0004-637X/814/2/109
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300027
ER
PT J
AU Barnes, R
Meadows, VS
Evans, N
AF Barnes, Rory
Meadows, Victoria S.
Evans, Nicole
TI COMPARATIVE HABITABILITY OF TRANSITING EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: surfaces
ID MAIN-SEQUENCE STARS; EARTH-LIKE EXOPLANETS; MULTI-PLANET SYSTEMS;
WEBB-SPACE-TELESCOPE; SUN-LIKE STARS; M DWARFS; SUPER-EARTHS; ORBITAL
ECCENTRICITIES; TERRESTRIAL PLANETS; EXTRASOLAR PLANET
AB Exoplanet habitability is traditionally assessed by comparing a planet's semimajor axis to the location of its host star's "habitable zone," the shell around a star for which Earth-like planets can possess liquid surface water. The Kepler space telescope has discovered numerous planet candidates near the habitable zone, and many more are expected from missions such as K2, TESS, and PLATO. These candidates often require significant follow-up observations for validation, so prioritizing planets for habitability from transit data has become an important aspect of the search for life in the universe. We propose a method to compare transiting planets for their potential to support life based on transit data, stellar properties and previously reported limits on planetary emitted flux. For a planet in radiative equilibrium, the emitted flux increases with eccentricity, but decreases with albedo. As these parameters are often unconstrained, there is an "eccentricity-albedo degeneracy" for the habitability of transiting exoplanets. Our method mitigates this degeneracy, includes a penalty for large-radius planets, uses terrestrial mass-radius relationships, and, when available, constraints on eccentricity to compute a number we call the "habitability index for transiting exoplanets" that represents the relative probability that an exoplanet could support liquid surface water. We calculate it for Kepler objects of interest and find that planets that receive between 60% and 90% of the Earth's incident radiation, assuming circular orbits, are most likely to be habitable. Finally, we make predictions for the upcoming TESS and James Webb Space Telescope missions.
C1 [Barnes, Rory; Meadows, Victoria S.; Evans, Nicole] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Barnes, Rory; Meadows, Victoria S.; Evans, Nicole] NASA, Astrobiol Inst, Virtual Planetary Lab, Lead Team, New York, NY USA.
RP Barnes, R (reprint author), Univ Washington, Dept Astron, Box 951580, Seattle, WA 98195 USA.
EM rory@astro.washington.edu
FU National Aeronautics and Space Administration under Exoplanet
Exploration Program; NASA Astrobiology Institute's Virtual Planet
Laboratory [NNA13AA93A]
FX We thank Pramod Gupta for designing the web interface that calculates
the HITE, and Eric Agol, Kevin Zahnle, Rodrigo Luger, Abel Mendez, Rene
Heller, Drake Deming, Mark Claire, and the entire Virtual Planetary
Laboratory for insightful discussions. 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. This work was
supported by the NASA Astrobiology Institute's Virtual Planet Laboratory
under Cooperative Agreement No. NNA13AA93A.
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 DEC 1
PY 2015
VL 814
IS 2
AR 91
DI 10.1088/0004-637X/814/2/91
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300009
ER
PT J
AU Bauer, JM
Stevenson, R
Kramer, E
Mainzer, AK
Grav, T
Masiero, JR
Fernandez, YR
Cutri, RM
Dailey, JW
Masci, FJ
Meech, KJ
Walker, R
Lisse, CM
Weissman, PR
Nugent, CR
Sonnett, S
Blair, N
Lucas, A
McMillan, RS
Wright, EL
AF Bauer, James M.
Stevenson, Rachel
Kramer, Emily
Mainzer, A. K.
Grav, Tommy
Masiero, Joseph R.
Fernandez, Yan R.
Cutri, Roc M.
Dailey, John W.
Masci, Frank J.
Meech, Karen J.
Walker, Russel
Lisse, C. M.
Weissman, Paul R.
Nugent, Carrie R.
Sonnett, Sarah
Blair, Nathan
Lucas, Andrew
McMillan, Robert S.
Wright, Edward L.
CA WISE Team
NEOWISE Team
TI THE NEOWISE-DISCOVERED COMET POPULATION AND THE CO + CO2 PRODUCTION
RATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; infrared: planetary systems
ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; NEAR-EARTH
ASTEROIDS; WISE/NEOWISE OBSERVATIONS; MAIN BELT; PHYSICAL-PROPERTIES;
NUCLEUS; PERFORMANCE; MISSION; ORIGIN
AB The 163 comets observed during the WISE/NEOWISE prime mission represent the largest infrared survey to date of comets, providing constraints on dust, nucleus size, and CO + CO2 production. We present detailed analyses of the WISE/NEOWISE comet discoveries, and discuss observations of the active comets showing 4.6 mu m band excess. We find a possible relation between dust and CO + CO2 production, as well as possible differences in the sizes of long and short period comet nuclei.
C1 [Bauer, James M.; Stevenson, Rachel; Kramer, Emily; Mainzer, A. K.; Masiero, Joseph R.; Weissman, Paul R.; Nugent, Carrie R.; Sonnett, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, James M.; Cutri, Roc M.; Dailey, John W.; Masci, Frank J.; Blair, Nathan; Lucas, Andrew] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Grav, Tommy] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Fernandez, Yan R.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Meech, Karen J.] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA.
[Meech, Karen J.] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, Manoa, HI 96822 USA.
[Walker, Russel] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McMillan, Robert S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM bauer@scn.jpl.nasa.gov
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Fernandez, Yanga/0000-0003-1156-9721;
Cutri, Roc/0000-0002-0077-2305; Kramer, Emily/0000-0003-0457-2519
FU National Aeronautics and Space Administration; Planetary Science
Division of NASA; NASA through NASA Astrobiology Institute [NNA09DA77A];
NASA Postdoctoral Program; NASA Earth and Space Science Fellowship
program
FX This publication makes use of data products from 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. This publication also makes use of data products from
NEOWISE, which is a project of JPL/Caltech, funded by the Planetary
Science Division of NASA. This material is based in part upon work
supported by the NASA through the NASA Astrobiology Institute under
Cooperative Agreement No. NNA09DA77A issued through the Office if Space
Science. R. Stevenson and E. Kramer were supported by the NASA
Postdoctoral Program, and E. Kramer acknowledges her support through the
NASA Earth and Space Science Fellowship program. We thank the
Astrophysical Journal Editor for the very helpful comments regarding
manuscript drafts, and the anonymous reviewer for providing valuable
comments, both of whom greatly improved the paper content. The lead
author also benefited greatly from a discussion with Nader Haghighipour
of the Institute for Astronomy and NASA Astrobiology Institute,
University of Hawaii-Manoa.
NR 56
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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 DEC 1
PY 2015
VL 814
IS 2
AR 85
DI 10.1088/0004-637X/814/2/85
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300003
ER
PT J
AU Miller, JM
Fabian, AC
Kaastra, J
Kallman, T
King, AL
Proga, D
Raymond, J
Reynolds, CS
AF Miller, J. M.
Fabian, A. C.
Kaastra, J.
Kallman, T.
King, A. L.
Proga, D.
Raymond, J.
Reynolds, C. S.
TI POWERFUL, ROTATING DISK WINDS FROM STELLAR-MASS BLACK HOLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries
ID X-RAY BINARIES; TRANSMISSION GRATING SPECTROMETER; ABSORPTION-LINES;
ACCRETION DISKS; GRS 1915+105; INTERSTELLAR-MEDIUM; WARM ABSORBERS;
CHANDRA HETGS; CYGNUS X-1; IRON LINE
AB We present an analysis of ionized X-ray disk winds found in the Fe K band of four stellar-mass black holes observed with Chandra, including 4U 1630-47, GRO J1655-40, H 1743-322, and GRS 1915+105. High-resolution photoionization grids were generated in order to model the data. Third-order gratings spectra were used to resolve complex absorption profiles into atomic effects and multiple velocity components. The Fe XXV line is found to be shaped by contributions from the intercombination line (in absorption), and the Fe XXVI line is detected as a spin-orbit doublet. The data require 2-3 absorption zones, depending on the source. The fastest components have velocities approaching or exceeding 0.01c, increasing mass outflow rates and wind kinetic power by orders of magnitude over prior single-zone models. The first-order spectra require re-emission from the wind, broadened by a degree that is loosely consistent with Keplerian orbital velocities at the photoionization radius. This suggests that disk winds are rotating with the orbital velocity of the underlying disk, and provides a new means of estimating launching radii-crucial to understanding wind driving mechanisms. Some aspects of the wind velocities and radii correspond well to the broad-line region in active galactic nuclei (AGNs), suggesting a physical connection. We discuss these results in terms of prevalent models for disk wind production and disk accretion itself, and implications for massive black holes in AGNs.
C1 [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, NL, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, NL-3508 TA Utrecht, Netherlands.
[Kallman, T.] NASA, Goddard Space Flight Ctr, Greedbelt, MD 20771 USA.
[King, A. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
OI Reynolds, Christopher/0000-0002-1510-4860
NR 72
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U2 2
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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 DEC 1
PY 2015
VL 814
IS 2
AR 87
DI 10.1088/0004-637X/814/2/87
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300005
ER
PT J
AU Mori, K
Hailey, CJ
Krivonos, R
Hong, J
Ponti, G
Bauer, F
Perez, K
Nynka, M
Zhang, S
Tomsick, JA
Alexander, DM
Baganoff, FK
Barret, D
Barriere, N
Boggs, SE
Canipe, AM
Christensen, FE
Craig, WW
Forster, K
Giommi, P
Grefenstette, BW
Grindlay, JE
Harrison, FA
Hornstrup, A
Kitaguchi, T
Koglin, JE
Luu, V
Madsen, KK
Mao, PH
Miyasaka, H
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, V
Stern, D
Westergaard, NJ
Zhang, WW
Zoglauer, A
AF Mori, Kaya
Hailey, Charles J.
Krivonos, Roman
Hong, Jaesub
Ponti, Gabriele
Bauer, Franz
Perez, Kerstin
Nynka, Melania
Zhang, Shuo
Tomsick, John A.
Alexander, David M.
Baganoff, Frederick K.
Barret, Didier
Barriere, Nicolas
Boggs, Steven E.
Canipe, Alicia M.
Christensen, Finn E.
Craig, William W.
Forster, Karl
Giommi, Paolo
Grefenstette, Brian W.
Grindlay, Jonathan E.
Harrison, Fiona A.
Hornstrup, Allan
Kitaguchi, Takao
Koglin, Jason E.
Luu, Vy
Madsen, Kristen K.
Mao, Peter H.
Miyasaka, Hiromasa
Perri, Matteo
Pivovaroff, Michael J.
Puccetti, Simonetta
Rana, Vikram
Stern, Daniel
Westergaard, Niels J.
Zhang, William W.
Zoglauer, Andreas
TI NuSTAR HARD X-RAY SURVEY OF THE GALACTIC CENTER REGION. I. HARD X-RAY
MORPHOLOGY AND SPECTROSCOPY OF THE DIFFUSE EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; radiation mechanisms: non-thermal; X-rays: general;
X-rays: ISM
ID SGR-A-ASTERISK; PULSAR WIND NEBULAE; ENERGY GAMMA-RAYS; SUPERMASSIVE
BLACK-HOLE; XMM-NEWTON OBSERVATIONS; KEV LINE EMISSION; SAGITTARIUS-A;
MOLECULAR CLOUDS; SUPERNOVA-REMNANT; COSMIC-RAYS
AB We present the first sub-arcminute images of the Galactic Center above 10 keV, obtained with NuSTAR. NuSTAR resolves the hard X-ray source IGR J17456-2901 into non-thermal X-ray filaments, molecular clouds, point sources, and a previously unknown central component of hard X-ray emission (CHXE). NuSTAR detects four non-thermal X-ray filaments, extending the detection of their power-law spectra with Gamma similar to 1.3-2.3 up to similar to 50 keV. A morphological and spectral study of the filaments suggests that their origin may be heterogeneous, where previous studies suggested a common origin in young pulsar wind nebulae (PWNe). NuSTAR detects non-thermal X-ray continuum emission spatially correlated with the 6.4 keV Fe K alpha fluorescence line emission associated with two Sgr A molecular clouds: MC1 and the Bridge. Broadband X-ray spectral analysis with a Monte-Carlo based X-ray reflection model self-consistently determined their intrinsic column density (similar to 10(23) cm(-2)), primary X-ray spectra (power-laws with Gamma similar to 2) and set a lower limit of the X-ray luminosity of Sgr A* flare illuminating the Sgr A clouds to L-X >= 10(38) erg s(-1). Above similar to 20 keV, hard X-ray emission in the central 10 pc region around Sgr A* consists of the candidate PWN G359.95-0.04 and the CHXE, possibly resulting from an unresolved population of massive CVs with white dwarf masses M-WD similar to 0.9M(circle dot). Spectral energy distribution analysis suggests that G359.95-0.04 is likely the hard X-ray counterpart of the ultra-high gamma-ray source HESS J1745-290, strongly favoring a leptonic origin of the GC TeV emission.
C1 [Mori, Kaya; Hailey, Charles J.; Perez, Kerstin; Nynka, Melania; Zhang, Shuo; Canipe, Alicia M.; Luu, Vy] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Krivonos, Roman; Tomsick, John A.; Barriere, Nicolas; Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Krivonos, Roman] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Hong, Jaesub; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ponti, Gabriele] Max Planck Inst Extraterr Phys, HEG, D-85748 Garching, Germany.
[Bauer, Franz] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, Franz] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, Franz] Space Sci Inst, Boulder, CO 80301 USA.
[Perez, Kerstin] Haverford Coll, Haverford, PA 19041 USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Barret, Didier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Christensen, Finn E.; Hornstrup, Allan; Westergaard, Niels J.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.; Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Forster, Karl; Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristen K.; Mao, Peter H.; Miyasaka, Hiromasa; Rana, Vikram] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Giommi, Paolo; Perri, Matteo; Puccetti, Simonetta] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Kitaguchi, Takao] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Kitaguchi, Takao] Hiroshima Univ, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan.
[Koglin, Jason E.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Perri, Matteo; Puccetti, Simonetta] INAF Astronom Roma, I-00040 Monte Porzio Catone, Italy.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mori, K (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM kaya@astro.columbia.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Puccetti,
Simonetta/0000-0002-2734-7835; Rana, Vikram/0000-0003-1703-8796;
Krivonos, Roman/0000-0003-2737-5673
FU NASA [NNG08FD60C]; Russian Science Foundation [14-22-00271]; EU Marie
Curie IntraEuropean fellowship [FP-PEOPLE-2012-IEF-331095];
Bundesministerium fur Wirtschaft und Technologie/DeutschesZentrum fur
Luf-und R fahrt (BMWI/DLR) [FKZ 50 OR 1408]; Max Planck Society;
CONICYT-Chile (Basal-CATA) [PFB-06/2007]; CONICYT-Chile (FONDECYT)
[1141218]; CONICYT-Chile ("EMBIGGEN" Anillo) [ACT1101]; Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
[IC120009]; NASA Headquarters under the NASA Earth and Space Science
Fellowship Program-Grant [NNX13AM31]; French Space Agency (CNES)
FX 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). R. Krivonos acknowledges support from
Russian Science Foundation through grant 14-22-00271. G. Ponti
acknowledges support via an EU Marie Curie IntraEuropean fellowship
under contract no. FP-PEOPLE-2012-IEF-331095, the Bundesministerium fur
Wirtschaft und Technologie/DeutschesZentrum fur Luf-und R fahrt
(BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. F.E. Bauer
acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007,
FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and the Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
through grant IC120009, awarded to The Millennium Institute of
Astrophysics, MAS. S. Zhang is supported by NASA Headquarters under the
NASA Earth and Space Science Fellowship Program-Grant "NNX13AM31." D.
Barret acknowledges support from the French Space Agency (CNES). We
thank Tahir Yaqoob for useful discussions on the MYTorus model.
NR 132
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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 DEC 1
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PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300012
ER
PT J
AU Novati, SC
Gould, A
Yee, JC
Beichman, C
Bryden, G
Carey, S
Fausnaugh, M
Gaudi, BS
Henderson, CB
Pogge, RW
Shvartzvald, Y
Wibking, B
Zhu, W
Udalski, A
Poleski, R
Pawlak, M
Szymanski, MK
Skowron, J
Mroz, P
Kozlowski, S
Wyrzykowski, L
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
AF Novati, S. Calchi
Gould, A.
Yee, J. C.
Beichman, C.
Bryden, G.
Carey, S.
Fausnaugh, M.
Gaudi, B. S.
Henderson, C. B.
Pogge, R. W.
Shvartzvald, Y.
Wibking, B.
Zhu, W.
Udalski, A.
Poleski, R.
Pawlak, M.
Szymanski, M. K.
Skowron, J.
Mroz, P.
Kozlowski, S.
Wyrzykowski, L.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
CA Spitzer Team
OGLE Grp
TI SPITZER IRAC PHOTOMETRY FOR TIME SERIES IN CROWDED FIELDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; techniques: photometric
ID GRAVITATIONAL LENSING EXPERIMENT; MAGNIFICATION MICROLENSING EVENTS;
PARALLAX SATELLITE MASS; EXTRASOLAR PLANET; GALACTIC BULGE; SYSTEMS;
STARS
AB We develop a new photometry algorithm that is optimized for the Infrared Array Camera (IRAC) Spitzer time series in crowded fields and that is particularly adapted to faint or heavily blended targets. We apply this to the 170 targets from the 2015 Spitzer microlensing campaign and present the results of three variants of this algorithm in an online catalog. We present detailed accounts of the application of this algorithm to two difficult cases, one very faint and the other very crowded. Several of Spitzer's instrumental characteristics that drive the specific features of this algorithm are shared by Kepler and WFIRST, implying that these features may prove to be a useful starting point for algorithms designed for microlensing campaigns by these other missions.
C1 [Novati, S. Calchi; Beichman, C.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi] Ist Int Alti Studi Sci, I-84019 Vietri Sul Mare, SA, Italy.
[Gould, A.; Fausnaugh, M.; Gaudi, B. S.; Henderson, C. B.; Pogge, R. W.; Wibking, B.; Zhu, W.; Udalski, A.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bryden, G.; Henderson, C. B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carey, S.] CALTECH, Ctr Sci, Spitzer, Pasadena, CA 91125 USA.
[Udalski, A.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
RP Novati, SC (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
RI Kozlowski, Szymon/G-4799-2013; Skowron, Jan/M-5186-2014;
OI Kozlowski, Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730;
Pogge, Richard/0000-0003-1435-3053
FU JPL grant [1500811]; NASA Postdoctoral Program at Jet Propulsion
Laboratory; NASA through Sagan Fellowship Program by NASA Exoplanet
Science Institute; NASA by JPL/Caltech; National Science Centre, Poland
[MAESTRO 2014/14/A/ST9/00121]
FX We thank J. Ingalls for a useful discussion about PRF fitting with IRAC
data. Work by S.C.N., A.G., S.C., J.C.Y., and W.Z. was supported by JPL
grant 1500811. 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. 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. 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 OGLE project has received funding
from the National Science Centre, Poland, grant MAESTRO
2014/14/A/ST9/00121 to AU.
NR 34
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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 DEC 1
PY 2015
VL 814
IS 2
AR 92
DI 10.1088/0004-637X/814/2/92
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300010
ER
PT J
AU Nugent, CR
Mainzer, A
Masiero, J
Bauer, J
Cutri, RM
Grav, T
Kramer, E
Sonnett, S
Stevenson, R
Wright, EL
AF Nugent, C. R.
Mainzer, A.
Masiero, J.
Bauer, J.
Cutri, R. M.
Grav, T.
Kramer, E.
Sonnett, S.
Stevenson, R.
Wright, E. L.
TI NEOWISE REACTIVATION MISSION YEAR ONE: PRELIMINARY ASTEROID DIAMETERS
AND ALBEDOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general
ID NEAR-EARTH ASTEROIDS; MAIN-BELT ASTEROIDS; INFRARED-SURVEY-EXPLORER;
PHYSICAL-PROPERTIES; WISE/NEOWISE OBSERVATIONS; THERMAL-MODEL; FAMILIES;
IDENTIFICATION; PERFORMANCE; PHOTOMETRY
AB We present preliminary diameters and albedos for 7956 asteroids detected in the first year of the NEOWISE Reactivation mission. Of those, 201 are near-Earth asteroids and 7755 are Main Belt or Mars-crossing asteroids. 17% of these objects have not been previously characterized using the Near-Earth Object Wide-field Infrared Survey Explorer, or "NEOWISE " thermal measurements. Diameters are determined to an accuracy of similar to 20% or better. If good-quality H magnitudes are available, albedos can be determined to within similar to 40% or better.
C1 [Nugent, C. R.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Mainzer, A.; Masiero, J.; Bauer, J.; Kramer, E.; Sonnett, S.; Stevenson, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Nugent, CR (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
EM cnugent@ipac.caltech.edu
OI Masiero, Joseph/0000-0003-2638-720X; Cutri, Roc/0000-0002-0077-2305;
Kramer, Emily/0000-0003-0457-2519
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory (JPL); NASA;
Planetary Science Division of NASA; JPL Office of the CIO; U.S.
Department of Energy; U.S. 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; 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
FX C.R.N. was partially supported by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory (JPL),
administered by Oak Ridge Associated Universities through a contract
with NASA. This publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and JPL/California Institute of
Technology, funded by NASA. This publication also makes use of data
products from NEOWISE, which is a project of the JPL/California
Institute of Technology, funded by the Planetary Science Division of
NASA. This research has made use of the NASA/IPAC Infrared Science
Archive. The JPL High-Performance Computing Facility used for our
simulations is supported by the JPL Office of the CIO.; This project
used data obtained with the Dark Energy Camera (DECam), which was
constructed by the Dark Energy Survey (DES) collaboration. Funding for
the DES Projects has been provided by the U.S. Department of Energy, the
U.S. 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 Dark Energy Survey. 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.
NR 46
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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 DEC 1
PY 2015
VL 814
IS 2
AR 117
DI 10.1088/0004-637X/814/2/117
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300035
ER
PT J
AU Prezeau, G
AF Prezeau, G.
TI DENSE DARK MATTER HAIRS SPREADING OUT FROM EARTH, JUPITER, AND OTHER
COMPACT BODIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter
ID PHASE-SPACE STRUCTURE; VELOCITY; GALAXIES; HALOES; MASS
AB It is shown that compact bodies project out strands of concentrated dark matter filaments, henceforth simply called hairs. These hairs are a consequence of the fine-grained stream structure of dark matter halos, and as such constitute a new physical prediction of Lambda CDM. Using both an analytical model of planetary density and numerical simulations utilizing the Fast Accurate Integrand Renormalization algorithm (a fast geodesics calculator described below) with realistic planetary density inputs, dark matter streams moving through a compact body are shown to produce hugely magnified dark matter densities along the stream velocity axis passing through the center of the body. Typical hair density enhancements are 10(7) for Earth and 10(8) for Jupiter. The largest enhancements occur for particles streaming through the core of the body that are mostly focused at a single point called the root of the hair. For the Earth, the root is located at about 10(6) km from the planetary center with a density enhancement of around 10(9) while for a gas giant like Jupiter, the root is located at around 10(5) km with an enhancement of around 10(11). Beyond the root, the hair density precisely reflects the density layers of the body, providing a direct probe of planetary interiors.
C1 [Prezeau, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Prezeau, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU internal Research and Technology Development program; NASA through the
US Planck collaboration
FX The author would like to thank Takeyasu Ito, Charles Lawrence, and Brad
Plaster for useful suggestions and comments. This research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration and funded through the internal Research and Technology
Development program. This work was also supported by NASA through the US
Planck collaboration. Government sponsorship acknowledged.
NR 35
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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 DEC 1
PY 2015
VL 814
IS 2
AR 122
DI 10.1088/0004-637X/814/2/122
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300040
ER
PT J
AU Shvartzvald, Y
Udalski, A
Gould, A
Han, C
Bozza, V
Friedmann, M
Hundertmark, M
Beichman, C
Bryden, G
Novati, SC
Carey, S
Fausnaugh, M
Gaudi, BS
Henderson, CB
Kerr, T
Pogge, RW
Varricatt, W
Wibking, B
Yee, JC
Zhu, W
Poleski, R
Pawlak, M
Szymanski, MK
Skowron, J
Mroz, P
Kozlowski, S
Wyrzykowski, L
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
Choi, JY
Park, H
Jung, YK
Shin, IG
Albrow, MD
Park, BG
Kim, SL
Lee, CU
Cha, SM
Kim, DJ
Lee, Y
Maoz, D
Kaspi, S
Street, RA
Tsapras, Y
Bachelet, E
Dominik, M
Bramich, DM
Horne, K
Snodgrass, C
Steele, IA
Menzies, J
Jaimes, RF
Wambsganss, J
Schmidt, R
Cassan, A
Ranc, C
Mao, S
Dong, SB
D'Ago, G
Scarpetta, G
Verma, P
Jorgensen, UG
Kerins, E
Skottfelt, J
AF Shvartzvald, Y.
Udalski, A.
Gould, A.
Han, C.
Bozza, V.
Friedmann, M.
Hundertmark, M.
Beichman, C.
Bryden, G.
Novati, S. Calchi
Carey, S.
Fausnaugh, M.
Gaudi, B. S.
Henderson, C. B.
Kerr, T.
Pogge, R. W.
Varricatt, W.
Wibking, B.
Yee, J. C.
Zhu, W.
Poleski, R.
Pawlak, M.
Szymanski, M. K.
Skowron, J.
Mroz, P.
Kozlowski, S.
Wyrzykowski, L.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
Choi, J. -Y.
Park, H.
Jung, Y. K.
Shin, I. -G.
Albrow, M. D.
Park, B. -G.
Kim, S. -L.
Lee, C. -U.
Cha, S. -M.
Kim, D. -J.
Lee, Y.
Maoz, D.
Kaspi, S.
Street, R. A.
Tsapras, Y.
Bachelet, E.
Dominik, M.
Bramich, D. M.
Horne, Keith
Snodgrass, C.
Steele, I. A.
Menzies, J.
Jaimes, R. Figuera
Wambsganss, J.
Schmidt, R.
Cassan, A.
Ranc, C.
Mao, S.
Dong, Subo
D'Ago, G.
Scarpetta, G.
Verma, P.
Jorgensen, U. G.
Kerins, E.
Skottfelt, J.
CA Spitzer Team
OGLE Grp
KMTNet Grp
Wise Grp
RoboNet
MiNDSTEp
TI SPITZER MICROLENS MEASUREMENT OF A MASSIVE REMNANT IN A WELL-SEPARATED
BINARY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; black hole physics; Galaxy: bulge; gravitational
lensing: micro; stars: neutron
ID GRAVITATIONAL LENSING EXPERIMENT; PARALLAX SATELLITE MASS; GALACTIC
BULGE; PROPER MOTIONS; OGLE-III; ASTROMETRY; STARS; PHOTOMETRY; PLANETS;
DISTANCE
AB We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La, b, with the more massive component having M-1 > 1.35M(circle dot) (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r(perpendicular to) = 6.1 +/- 0.4 AU and lies in the Galactic bulge. These measurements are based on the "microlens parallax" effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.
C1 [Shvartzvald, Y.; Bryden, G.; Henderson, C. B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Udalski, A.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Gould, A.; Fausnaugh, M.; Gaudi, B. S.; Henderson, C. B.; Pogge, R. W.; Wibking, B.; Zhu, W.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Han, C.; Choi, J. -Y.; Park, H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Friedmann, M.; Maoz, D.; Kaspi, S.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Hundertmark, M.; Jorgensen, U. G.] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M.; Jorgensen, U. G.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Beichman, C.; Novati, S. Calchi] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, S. Calchi; D'Ago, G.; Scarpetta, G.; Verma, P.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, S.] CALTECH, Ctr Sci, Spitzer, Pasadena, CA 91125 USA.
[Kerr, T.; Varricatt, W.] UKIRT, Hilo, HI 96720 USA.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Park, B. -G.; Kim, S. -L.; Lee, C. -U.; Cha, S. -M.; Kim, D. -J.; Lee, Y.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea.
[Cha, S. -M.; Kim, D. -J.; Lee, Y.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
[Street, R. A.; Bachelet, E.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Tsapras, Y.; Wambsganss, J.; Schmidt, R.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Bachelet, E.; Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar.
[Dominik, M.; Horne, Keith; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[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.
[Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Jaimes, R. Figuera] European So Observ, D-85748 Garching, Germany.
[Cassan, A.; Ranc, C.] UPMC, Univ Paris 04, F-75014 Paris, France.
[Cassan, A.; Ranc, C.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Mao, S.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Mao, S.] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China.
[Mao, S.] Chinese Acad Sci, Natl Astron Observatories, Beijing 100012, Peoples R China.
[Mao, S.; Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
RP Shvartzvald, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Ranc, Clement/B-1958-2016; D'Ago, Giuseppe/N-8318-2016; Kozlowski,
Szymon/G-4799-2013; Skowron, Jan/M-5186-2014;
OI Ranc, Clement/0000-0003-2388-4534; D'Ago, Giuseppe/0000-0001-9697-7331;
Kozlowski, Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730;
Dominik, Martin/0000-0002-3202-0343; Snodgrass,
Colin/0000-0001-9328-2905
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; National
Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; JPL grant
[1500811]; NASA through the Sagan Fellowship Program; Creative Research
Initiative Program of National Research Foundation of Korea
[20090081561]; Polish NCN Harmonia [2012/06/M/ST9/00172]; US Israel
Binational Science Foundation; I-CORE program of the Israel Science
Foundation; Planning and Budgeting Committee; NPRP grant from the Qatar
National Research Fund [X-019-1-006]; Strategic Priority Research
Program-The Emergence of Cosmological Structures" of the Chinese Academy
of Sciences [XDB09000000]; Strategic Priority Research Program "The
Emergence of Cosmological Structures" of the Chinese Academy of Sciences
[XDB09000000]; National Natural Science Foundation of China (NSFC)
[11333003, 11390372]; Villum Foundation; NASA
FX 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. The OGLE project
has received funding from the National Science Centre, Poland, grant
MAESTRO 2014/14/A/ST9/00121 to AU. Work by J.C.Y., A.G., and S.C. was
supported by JPL grant 1500811. 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. Work by C.H.
was supported by Creative Research Initiative Program (20090081561) of
National Research Foundation of Korea. This research has made the
telescopes of KMTNet operated by the Korea Astronomy and Space Science
Institute (KASI). L.W. acknowledges support from the Polish NCN Harmonia
grant No. 2012/06/M/ST9/00172. D.M. and A.G. acknowledge support by a
grant from the US Israel Binational Science Foundation. Work by D.M. is
supported by the I-CORE program of the Israel Science Foundation and the
Planning and Budgeting Committee. This publication was made possible by
NPRP grant # X-019-1-006 from the Qatar National Research Fund (a member
of Qatar Foundation) S.D. is supported by "the Strategic Priority
Research Program-The Emergence of Cosmological Structures" of the
Chinese Academy of Sciences (grant No. XDB09000000). 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. 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. 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. The
United Kingdom Infrared Telescope (UKIRT) is supported by NASA and
operated under an agreement among the University of Hawaii, the
University of Arizona, and Lockheed Martin Advanced Technology Center;
operations are enabled through the cooperation of the Joint Astronomy
Centre of the Science and Technology Facilities Council of the U.K. This
work makes use of observations from the LCOGT network, which includes
three SUPAscopes owned by the University of St Andrews. The RoboNet
programme is an LCOGT Key Project using time allocations from the
University of St Andrews, LCOGT, and the University of Heidelberg
together with time on the Liverpool Telescope through the Science and
Technology Facilities Council (STFC), UK. This research has made use of
the LCOGT Archive, which is operated by the California Institute of
Technology, under contract with the Las Cumbres Observatory. 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.
NR 51
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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 DEC 1
PY 2015
VL 814
IS 2
AR 111
DI 10.1088/0004-637X/814/2/111
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300029
ER
PT J
AU Straughn, AN
Voyer, EN
Eufrasio, RT
de Mello, D
Petty, S
Kassin, S
Gardner, JP
Ravindranath, S
Soto, E
AF Straughn, Amber N.
Voyer, Elysse N.
Eufrasio, Rafael T.
de Mello, Duilia
Petty, Sara
Kassin, Susan
Gardner, Jonathan P.
Ravindranath, Swara
Soto, Emmaris
TI A MULTIWAVELENGTH STUDY OF TADPOLE GALAXIES IN THE HUBBLE ULTRA DEEP
FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: irregular
ID STAR-FORMING GALAXIES; EXTRAGALACTIC LEGACY SURVEY; LYMAN-BREAK
GALAXIES; FORMATION HISTORY; GOODS-SOUTH; CANDELS; MORPHOLOGIES;
EVOLUTION; RELEASE
AB Multiwavelength data are essential in order to provide a complete picture of galaxy evolution and to inform studies of galaxies' morphological properties across cosmic time. Here we present the results of a multiwavelength investigation of the morphologies of "tadpole" galaxies at intermediate redshift (0.314 < z < 3.175) in the Hubble Ultra Deep Field. These galaxies were previously selected from deep Hubble Space Telescope (HST) F775W data based on their distinct asymmetric knot-plus-tail morphologies. Here we use deep Wide Field Camera 3 near-infrared imaging in addition to the HST optical data in order to study the rest-frame UV/optical morphologies of these galaxies across the redshift range 0.3 < z < 3.2. This study reveals that the majority of these galaxies do retain their general asymmetric morphology in the rest-frame optical over this redshift range, if not the distinct "tadpole" shape. The average stellar mass of tadpole galaxies is lower than that of field galaxies, with the effect being slightly greater at higher redshift within the errors. Estimated from spectral energy distribution fits, the average age of tadpole galaxies is younger than that of field galaxies in the lower-redshift bin, and the average metallicity is lower (whereas the specific star formation rate for tadpoles is roughly the same as field galaxies across the redshift range probed here). These average effects combined support the conclusion that this subset of galaxies is in an active phase of assembly, either late-stage merging or cold gas accretion causing localized clumpy star formation.
C1 [Straughn, Amber N.; Eufrasio, Rafael T.; Gardner, Jonathan P.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Voyer, Elysse N.] Google, Randstad, Palo Alto, CA USA.
[Eufrasio, Rafael T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[de Mello, Duilia; Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Petty, Sara] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Kassin, Susan; Ravindranath, Swara] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Straughn, AN (reprint author), Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
RI Eufrasio, Rafael/F-7611-2016;
OI Eufrasio, Rafael/0000-0002-2987-1796; Kassin, Susan/0000-0002-3838-8093;
Soto, Emmaris/0000-0002-2390-0584
NR 44
TC 1
Z9 1
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 DEC 1
PY 2015
VL 814
IS 2
AR 97
DI 10.1088/0004-637X/814/2/97
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300015
ER
PT J
AU Watts, DJ
Larson, D
Marriage, TA
Abitbol, MH
Appel, JW
Bennett, CL
Chuss, DT
Eimer, JR
Essinger-Hileman, T
Miller, NJ
Rostem, K
Wollack, EJ
AF Watts, Duncan J.
Larson, David
Marriage, Tobias A.
Abitbol, Maximilian H.
Appel, John W.
Bennett, Charles L.
Chuss, David T.
Eimer, Joseph R.
Essinger-Hileman, Thomas
Miller, Nathan J.
Rostem, Karwan
Wollack, Edward J.
TI MEASURING THE LARGEST ANGULAR SCALE CMB B-MODE POLARIZATION WITH
GALACTIC FOREGROUNDS ON A CUT SKY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; early universe;
gravitational waves; inflation
ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND POLARIZATION; INFLATIONARY
UNIVERSE; SYMMETRY-BREAKING; POWER SPECTRA; EMISSION; ALGORITHM;
FLATNESS; HORIZON; MAPS
AB We consider the effectiveness of foreground cleaning in the recovery of Cosmic Microwave Background (CMB) polarization sourced by gravitational waves for tensor-to-scalar ratios in the range 0 < r < 0.1. Using the planned survey area, frequency bands, and sensitivity of the Cosmology Large Angular Scale Surveyor (CLASS), we simulate maps of Stokes Q and U parameters at 40, 90, 150, and 220 GHz, including realistic models of the CMB, diffuse Galactic thermal dust and synchrotron foregrounds, and Gaussian white noise. We use linear combinations (LCs) of the simulated multifrequency data to obtain maximum likelihood estimates of r, the relative scalar amplitude s, and LC coefficients. We find that for 10,000 simulations of a CLASS-like experiment using only measurements of the reionization peak (l <= 23), there is a 95% C. L. upper limit of r < 0.017 in the case of no primordial gravitational waves. For simulations with r = 0.01, we recover at 68% C. L. = r 0.012(-0.006)(+0.011) The reionization peak corresponds to a fraction of the multipole moments probed by CLASS, and simulations including 30. l. 100 further improve our upper limits to r < 0.008 at 95% C. L. (r = 0.010(-0.004)(+0.004) for primordial gravitational waves with r. =. 0.01). In addition to decreasing the current upper bound on r by an order of magnitude, these foreground-cleaned low multipole data will achieve a cosmic variance limited measurement of the E-mode polarization's reionization peak.
C1 [Watts, Duncan J.; Larson, David; Marriage, Tobias A.; Abitbol, Maximilian H.; Appel, John W.; Bennett, Charles L.; Eimer, Joseph R.; Essinger-Hileman, Thomas; Rostem, Karwan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21287 USA.
[Abitbol, Maximilian H.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Chuss, David T.] Villanova Univ, Dept Phys, Villanova, PA 19085 USA.
[Chuss, David T.; Miller, Nathan J.; Rostem, Karwan; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Watts, DJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3701 San Martin Dr, Baltimore, MD 21287 USA.
EM dwatts@jhu.edu
RI Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Watts, Duncan/0000-0002-5437-6121
FU National Science Foundation Division of Astronomical Sciences [0959349,
1429236]; NASA [NNX14AB76A]; Comision Nacional de Investigacion
Cientifica y Tecnologica de Chile (CONICYT); Maryland Space Grant
Consortium; National Science Foundation Astronomy and Astrophysics
Postdoctoral Fellowship
FX We acknowledge the National Science Foundation Division of Astronomical
Sciences for their support of CLASS under Grant Numbers 0959349 and
1429236. The CLASS project developed technology under several previous
NASA grants, and NASA provides ongoing detector support for civil
servants. Detector development work at JHU was funded by NASA grant
number NNX14AB76A. CLASS is located in the Parque Astronomica Atacama in
northern Chile under the auspices of the Comision Nacional de
Investigacion Cientifica y Tecnologica de Chile (CONICYT). D. J. W.
receives support from the Maryland Space Grant Consortium. T. E.-H.
receives support from a National Science Foundation Astronomy and
Astrophysics Postdoctoral Fellowship. Our analysis used the numpy (van
der Walt et al. 2011), scipy (Jones et al. 2001), and matplotlib (Hunter
2007) packages in Python. Some of the results in this paper have been
derived using the HEALPix (Gorski et al. 2005) package. This research
project was conducted using computational resources at the Maryland
Advanced Research Computing Center (MARCC).
NR 55
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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 DEC 1
PY 2015
VL 814
IS 2
AR 103
DI 10.1088/0004-637X/814/2/103
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300021
ER
PT J
AU Webb, TMA
Muzzin, A
Noble, A
Bonaventura, N
Geach, J
Hezevah, Y
Lidman, C
Wilson, G
Yee, HKC
Surace, J
Shupe, D
AF Webb, Tracy M. A.
Muzzin, Adam
Noble, Allison
Bonaventura, Nina
Geach, James
Hezevah, Yashar
Lidman, Chris
Wilson, Gillian
Yee, H. K. C.
Surace, Jason
Shupe, David
TI THE STAR FORMATION HISTORY OF BCGs TO z=1.8 FROM THE SpARCS/SWIRE
SURVEY: EVIDENCE FOR SIGNIFICANT IN SITU STAR FORMATION AT HIGH REDSHIFT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: formation;
galaxies: star formation
ID BRIGHTEST CLUSTER GALAXIES; ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC LEGACY
SURVEY; SIMILAR-TO 1; MASSIVE GALAXIES; SPECTROSCOPIC CONFIRMATION;
COOLING FLOWS; MOLECULAR GAS; STELLAR MASS; PHOTOMETRIC REDSHIFTS
AB We present the results of an MIPS-24 mu m study of the brightest cluster galaxies (BCGs) of 535 high-redshift galaxy clusters. The clusters are drawn from the Spitzer Adaptation of the Red-Sequence Cluster Survey, which effectively provides a sample selected on total stellar mass, over 0.2 < z < 1.8 within the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey fields. Twenty percent, or 106 clusters, have spectroscopically confirmed redshifts, and the rest have redshifts estimated from the color of their red sequence. A comparison with the public SWIRE images detects 125 individual BCGs at 24 mu m greater than or similar to 100 mu Jy, or 23%. The luminosity-limited detection rate of BCGs in similar richness clusters (N-gal > 12) increases rapidly with redshift. Above z similar to 1, an average of similar to 20% of the sample have 24 mu m inferred infrared luminosities of L-IR > 10(12) L-circle dot, while the fraction below z similar to 1 exhibiting such luminosities is <1%. The Spitzer-IRAC colors indicate the bulk of the 24 mu m detected population is predominantly powered by star formation, with only 7/125 galaxies lying within the color region inhabited by active galactic nuclei (AGNs). Simple arguments limit the star formation activity to several hundred million years and this may therefore be indicative of the timescale for AGN feedback to halt the star formation. Below redshift z similar to 1, there is not enough star formation to significantly contribute to the overall stellar mass of the BCG population, and therefore BCG growth is likely dominated by dry mergers. Above z similar to 1, however, the inferred star formation would double the stellar mass of the BCGs and is comparable to the mass assembly predicted by simulations through dry mergers. We cannot yet constrain the process driving the star formation for the overall sample, though a single object studied in detail is consistent with a gas-rich merger.
C1 [Webb, Tracy M. A.; Bonaventura, Nina] McGill Univ, Montreal, PQ H3A 2T8, Canada.
[Muzzin, Adam] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Noble, Allison; Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Geach, James] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Hezevah, Yashar] Stanford Univ, Kavli Inst Particle Phys & Cosmol, Stanford, CA 94305 USA.
[Lidman, Chris] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Wilson, Gillian] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Shupe, David] NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA.
RP Webb, TMA (reprint author), McGill Univ, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
FU NSF [AST-0607701, AST-0908246, AST-0908442, AST-0908354]; NASA
[Spitzer-1356708, 08-ADP08-0019, NNX09AC95G]; NSERC Discovery Grant;
Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science; NASA from the Space Telescope Science
Institute [GO-13306, GO-13677, GO-13747, GO-13845, GO-14327, NAS
5-26555]
FX Funding for PRIMUS is provided by NSF (AST-0607701, AST-0908246,
AST-0908442, AST-0908354) and NASA (Spitzer-1356708, 08-ADP08-0019,
NNX09AC95G). T.M.A.W. acknowledges the support of an NSERC Discovery
Grant. 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. Financial support for this work was provided by NASA through
programs GO-13306, GO-13677, GO-13747, GO-13845, and GO-14327 from the
Space Telescope Science Institute, which is operated by AURA, Inc.,
under NASA contract NAS 5-26555.
NR 82
TC 7
Z9 7
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 DEC 1
PY 2015
VL 814
IS 2
AR 96
DI 10.1088/0004-637X/814/2/96
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300014
ER
PT J
AU Yan, L
Quimby, R
Ofek, E
Gal-Yam, A
Mazzali, P
Perley, D
Vreeswijk, PM
Leloudas, G
de Cia, A
Masci, F
Cenko, SB
Cao, Y
Kulkarni, SR
Nugent, PE
Rebbapragada, UD
Wozniak, PR
Yaron, O
AF Yan, Lin
Quimby, R.
Ofek, E.
Gal-Yam, A.
Mazzali, P.
Perley, D.
Vreeswijk, P. M.
Leloudas, G.
de Cia, A.
Masci, F.
Cenko, S. B.
Cao, Y.
Kulkarni, S. R.
Nugent, P. E.
Rebbapragada, Umaa D.
Wozniak, P. R.
Yaron, O.
TI DETECTION OF BROAD H alpha EMISSION LINES IN THE LATE-TIME SPECTRA OF A
HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (iPTF13ehe, SN2007bi,
PTF12dam)
ID PULSATIONAL PAIR-INSTABILITY; GAMMA-RAY BURSTS; LUMINOUS SUPERNOVAE; IC
SUPERNOVAE; MAGNETIC-FIELDS; POPULATION III; LIGHT-CURVE; GALAXIES;
STARS; EXPLOSIONS
AB iPTF13ehe is a hydrogen-poor superluminous supernova (SLSN) at z = 0.3434, with a slow-evolving light curve and spectral features similar to SN2007bi. It rises in 83-148 days to reach a peak bolometric luminosity of similar to 1.3 x 10(44) erg s(-1), then decays slowly at 0.015 mag day(-1). The measured ejecta velocity is similar to 13,000 km s(-1). The inferred explosion characteristics, such as the ejecta mass (70-220M(circle dot)), and the total radiative and kinetic energy (E-rad similar to 10(51) erg, E-kin similar to 2 x 10(53) erg), are typical of slow-evolving H-poor SLSN events. However, the late-time spectrum taken at +251 days (rest, post-peak) reveals a Balmer Ha emission feature with broad and narrow components, which has never been detected before among other H-poor SLSNe. The broad component has a velocity width of similar to 4500 km s(-1) and a similar to 300 km s(-1) blueward shift relative to the narrow component. We interpret this broad Ha emission with a luminosity of similar to 2 x 10(41) erg s(-1) as resulting from the interaction between the supernova ejecta and a discrete H-rich shell, located at a distance of similar to 4 x 1016 cm from the explosion site. This interaction causes the rest-frame r-band LC to brighten at late times. The fact that the late-time spectra are not completely absorbed by the shock-ionized H-shell implies that its Thomson scattering optical depth is likely. 1, thus setting upper limits on the shell mass <= 30M(circle dot). Of the existing models, a Pulsational Pair Instability supernova model can naturally explain the observed 30M(circle dot) H-shell, ejected from a progenitor star with an initial mass of (95-150) M-circle dot about 40 years ago. We estimate that at least similar to 15% of all SLSNe-I may have late-time Balmer emission lines.
C1 [Yan, Lin; Masci, F.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Quimby, R.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Quimby, R.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Ofek, E.; Gal-Yam, A.; Vreeswijk, P. M.; Leloudas, G.; de Cia, A.; Yaron, O.] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Mazzali, P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Mazzali, P.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Perley, D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Perley, D.; Leloudas, G.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Cenko, S. B.] 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.
[Cao, Y.; Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wozniak, P. R.] Los Alamos Natl Lab, Space & Remote Sensing, Los Alamos, NM 87545 USA.
RP Yan, L (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
EM lyan@ipac.caltech.edu
OI Wozniak, Przemyslaw/0000-0002-9919-3310
FU EU/FP7 via ERC [307260]; Quantum universe I-Core program, Israeli
Committee for planning and budgeting; ISF; Minerva; Weizmann-UK "making
connections" program; Kimmel award; ARCHES award; Danish National
Research Foundation; Discovery Communications; National Science
Foundation [AST-1005313]; US Department of Energy, Laboratory Directed
Research and Development program; US Government; W. M. Keck Foundation
FX We thank the anonymous referee for the positive and constructive
suggestions, which have helped to improve the paper. We benefited from
discussions with Nick Scoville and Orly Gnat on collisional excitations
in ISM. We thank Mansi Kasliwal, Thomas Prince, and Howard Bond for
helping us obtain the P200 photometry at one epoch. Vicki Toy and John
Capone from University of Maryland are acknowledged for taking the
photometry observation using LMI on DCT. A.G.Y. is supported by EU/FP7
via ERC grant No. 307260, the Quantum universe I-Core program by the
Israeli Committee for planning and budgeting and the ISF; by Minerva and
ISF grants; by the Weizmann-UK "making connections" program; and by
Kimmel and ARCHES awards. The Dark Cosmology Centre is funded by the
Danish National Research Foundation. This paper made use of Lowell
Observatory's Discovery Channel Telescope (DCT). Lowell operates the DCT
in partnership with Boston University, Northern Arizona University, the
University of Maryland, and the University of Toledo. Partial support of
the DCT was provided by Discovery Communications. The Large Monolithic
Imager (LMI) on DCT was built by Lowell Observatory using funds from the
National Science Foundation (AST-1005313). LANL participation in iPTF is
supported by the US Department of Energy as a part of the Laboratory
Directed Research and Development program. A portion of this work was
carried out at the Jet Propulsion Laboratory under a Research and
Technology Development Grant, under contract with the National
Aeronautics and Space Administration. US Government support is
acknowledged. 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. 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 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. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 66
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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 DEC 1
PY 2015
VL 814
IS 2
AR 108
DI 10.1088/0004-637X/814/2/108
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300026
ER
PT J
AU Zhu, W
Gould, A
Beichman, C
Novati, SC
Carey, S
Gaudi, BS
Henderson, CB
Penny, M
Shvartzvald, Y
Yee, JC
Udalski, A
Poleski, R
Skowron, J
Kozlowski, S
Mroz, P
Pietrukowicz, P
Pietrzynski, G
Szymanski, MK
Soszynski, I
Ulaczyk, K
Wyrzykowski, L
Abe, F
Barry, RK
Bennett, DP
Bhattacharya, A
Bond, IA
Freeman, M
Fukui, A
Hirao, Y
Itow, Y
Koshimoto, N
Ling, H
Masuda, K
Matsubara, Y
Muraki, Y
Nagakane, M
Ohnishi, K
Saito, T
Sullivan, DJ
Sumi, T
Suzuki, D
Tristram, PJ
Rattenbury, N
Wakiyama, Y
Yonehara, A
Maoz, D
Kaspi, S
Friedmann, M
AF Zhu, Wei
Gould, Andrew
Beichman, Charles
Novati, Sebastiano Calchi
Carey, Sean
Gaudi, B. Scott
Henderson, Calen B.
Penny, Matthew
Shvartzvald, Yossi
Yee, Jennifer C.
Udalski, A.
Poleski, R.
Skowron, J.
Kozlowski, S.
Mroz, P.
Pietrukowicz, P.
Pietrzynski, G.
Szymanski, M. K.
Soszynski, I.
Ulaczyk, K.
Wyrzykowski, L.
Abe, F.
Barry, R. K.
Bennett, D. P.
Bhattacharya, A.
Bond, I. A.
Freeman, M.
Fukui, A.
Hirao, Y.
Itow, Y.
Koshimoto, N.
Ling, H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagakane, M.
Ohnishi, K.
Saito, To.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Tristram, P. J.
Rattenbury, N.
Wakiyama, Y.
Yonehara, A.
Maoz, D.
Kaspi, S.
Friedmann, M.
CA OGLE Collaboration
MOA Collaboration
Wise Grp
TI PLANET SENSITIVITY FROM COMBINED GROUND- AND SPACE-BASED MICROLENSING
OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID PARALLAX SATELLITE MASS; SPITZER OBSERVATIONS; EXTRASOLAR PLANETS;
MAGNIFICATION; COMPANIONS; STAR; LENS; SYSTEMS; EVENTS; FREQUENCY
AB To move one step forward toward a Galactic distribution of planets, we present the first planet sensitivity analysis for microlensing events with simultaneous observations from space and the ground. We present this analysis for two such events, OGLE-2014-BLG-0939 and OGLE-2014-BLG-0124, which both show substantial planet sensitivity even though neither of them reached high magnification. This suggests that an ensemble of low to moderate magnification events can also yield significant planet sensitivity, and therefore probability, for detecting planets. The implications of our results to the ongoing and future space-based microlensing experiments to measure the Galactic distribution of planets are discussed.
C1 [Zhu, Wei; Gould, Andrew; Gaudi, B. Scott; Henderson, Calen B.; Penny, Matthew; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Beichman, Charles; Novati, Sebastiano Calchi] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, Sebastiano Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Novati, Sebastiano Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, Sean] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Henderson, Calen B.; Shvartzvald, Yossi] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Yee, Jennifer C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Udalski, A.; Poleski, R.; Skowron, J.; Kozlowski, S.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Abe, F.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Wakiyama, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Barry, R. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Bond, I. A.; Ling, H.] Massey Univ, North Shore Mail Ctr, Inst Informat & Math Sci, Auckland, New Zealand.
[Freeman, M.; Rattenbury, N.] Univ Auckland, Dept Phys, Auckland 1, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan.
[Hirao, Y.; Koshimoto, N.; Nagakane, M.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand.
[Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kyoto 6038555, Japan.
[Maoz, D.; Kaspi, S.; Friedmann, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
RP Zhu, W (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
EM weizhu@astronomy.ohio-state.edu
RI Kozlowski, Szymon/G-4799-2013; Skowron, Jan/M-5186-2014;
OI Kozlowski, Szymon/0000-0003-4084-880X; Skowron, Jan/0000-0002-2335-1730;
ZHU, WEI/0000-0003-4027-4711
FU JPL [1500811]; NASA through the Sagan Fellowship Program; NASA; National
Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; [JSPS23103002];
[JSPS24253004]; [JSPS26247023]; [JSPS25103508]; [23340064]
FX Work by W.Z. and A.G. was supported by JPL grant 1500811. Work by J.C.Y.
and M.P. 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. Work by Y.S. is 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. The
OGLE project has received funding from the National Science Centre,
Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. T.S. acknowledges the
financial support from JSPS23103002, JSPS24253004, and JSPS26247023. The
MOA project is supported by the grant JSPS25103508 and 23340064. 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.
NR 40
TC 5
Z9 5
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 DEC 1
PY 2015
VL 814
IS 2
AR 129
DI 10.1088/0004-637X/814/2/129
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CW9KJ
UT WOS:000365317300047
ER
PT J
AU Shirazi-Fard, Y
Alwood, JS
Schreurs, AS
Castillo, AB
Globus, RK
AF Shirazi-Fard, Yasaman
Alwood, Joshua S.
Schreurs, Ann-Sofie
Castillo, Alesha B.
Globus, Ruth K.
TI Mechanical loading causes site-specific anabolic effects on bone
following exposure to ionizing radiation
SO BONE
LA English
DT Article
DE Mechanical loading; Ionizing radiation; Spaceflight; Histomorphometry;
Cancellous bone microarchitecture; Cortical bone; Bone marrow;
Osteoprogenitor; Stem cells
ID LONG-DURATION SPACEFLIGHT; TOTAL-BODY IRRADIATION; CORTICAL BONE;
CANCELLOUS BONE; TRABECULAR BONE; TIBIAL COMPRESSION; MUSCULOSKELETAL
DISUSE; FUNCTIONAL ADAPTATION; ADAPTIVE RESPONSE; CHILDHOOD-CANCER
AB During spaceflight, astronauts will be exposed to a complex mixture of ionizing radiation that poses a risk to their health. Exposure of rodents to ionizing radiation on Earth causes bone loss and increases osteoclasts in cancellous tissue, but also may cause persistent damage to stem cells and osteoprogenitors. We hypothesized that ionizing radiation damages skeletal tissue despite a prolonged recovery period, and depletes the ability of cells in the osteoblast lineage to respond at a later time. The goal of the current study was to test if irradiation prevents bone accrual and bone formation induced by an anabolic mechanical stimulus. Tibial axial compression was used as an anabolic stimulus after irradiation with heavy ions. Mice (male, C57BL/6J, 16 weeks) were exposed to high atomic number, high energy (HZE) iron ions (Fe-56, 2 Gy, 600 MeV/ion) (IR, n = 5) or sham-irradiated (Sham, n = 5). In vivo axial loading was initiated 5 months post-irradiation; right tibiae in anesthetized mice were subjected to an established protocol known to stimulate bone formation (cyclic 9N compressive pulse, 60 cycles/day, 3 day/wk for 4 weeks). In vivo data showed no difference due to irradiation in the apparent stiffness of the lower limb at the initiation of the axial loading regimen. Axial loading increased cancellous bone volume by microcomputed tomography and bone formation rate by histomorphometry in both sham and irradiated animals, with a main effect of axial loading determined by two-factor ANOVA with repeated measure. There were no effects of radiation in cancellous bone microarchitecture and indices of bone formation. At the tibia diaphysis, results also revealed a main effect of axial loading on structure. Furthermore, irradiation prevented axial loading-induced stimulation of bone formation rate at the periosteal surface of cortical tissue. In summary, axial loading stimulated the net accrual of cancellous and cortical mass and increased cancellous bone formation rate despite prior exposure to ionizing radiation, in this case, HZE particles. Our findings suggest that mechanical stimuli may prove an effective treatment to improve skeletal structure following exposure to ionizing radiation. Published by Elsevier Inc.
C1 [Shirazi-Fard, Yasaman; Alwood, Joshua S.; Schreurs, Ann-Sofie; Globus, Ruth K.] NASA, Ames Res Ctr, Bone & Signaling Lab, Space Biosci Div, Moffett Field, CA 94035 USA.
[Castillo, Alesha B.] NYU, Dept Mech & Aerosp Engn, New York, NY USA.
RP Globus, RK (reprint author), NASA, Ames Res Ctr, Mail Stop 236-7, Moffett Field, CA 94035 USA.
EM Yasaman.Shirazi-Fard@nasa.gov; joshua.s.alwood@nasa.gov;
ann-sofie.schreurs@nasa.gov; alesha.castillo@nyu.edu;
ruth.k.globus@nasa.gov
RI Schreurs, Ann-Sofie/A-5808-2016
OI Shirazi-Fard, Yasaman/0000-0002-6520-3824; Schreurs,
Ann-Sofie/0000-0002-9503-032X
FU National Space Biomedical Research Institute [NCC 9-58, MA02501]
FX This work is supported by the National Space Biomedical Research
Institute through NCC 9-58, grant MA02501. The authors gratefully
acknowledge members of Bone and Signaling Laboratory Tiffany Truong,
Eric Moyer, Samantha Torres, Kevin Bruns, and Mohit Nalavadi at NASA
Ames Research Center for their technical help and valuable contribution
during this project. The authors thank Brookhaven National Laboratory
Animal Care Facility and NASA Space Radiation Laboratory (NSRL) staff
Peter Guida, Adam Rusek, Michael Sivert, MaryAnn Petty, Kerry Bonti,
Angela Kim, and Laura Loudenslager for their assistance with this
experiment. Gratitude is extended to Matthew Silva and Michael Brodt at
Washington University Department of Orthopedic Surgery for expert
technical assistance with the axial compression design. Authors
gratefully acknowledge Peter Delisser and Joanna Price at University of
Bristol for their assistance with axial loading protocol, Matthew Allen
at Indiana University School of Medicine for histomorphometry analysis,
and Robert Ploutz-Snyder at NASA Johnson Space Center for advice on
statistical analyses.
NR 73
TC 2
Z9 2
U1 0
U2 3
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 8756-3282
EI 1873-2763
J9 BONE
JI Bone
PD DEC
PY 2015
VL 81
BP 260
EP 269
DI 10.1016/j.bone.2015.07.019
PG 10
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA CX0FR
UT WOS:000365372800033
PM 26191778
ER
PT J
AU Smith, SM
Heer, M
Shackelford, LC
Sibonga, JD
Spatz, J
Pietrzyk, RA
Hudson, EK
Zwart, SR
AF Smith, Scott M.
Heer, Martina
Shackelford, Linda C.
Sibonga, Jean D.
Spatz, Jordan
Pietrzyk, Robert A.
Hudson, Edgar K.
Zwart, Sara R.
TI Bone metabolism and renal stone risk during International Space Station
missions
SO BONE
LA English
DT Article
DE Biochemical markers of bone turnover; Exercise; Anti-resorptives
ID LONG-DURATION SPACEFLIGHT; BODY NEGATIVE-PRESSURE; HUMAN
SKELETAL-MUSCLE; BED REST; RESISTANCE EXERCISE; TREADMILL EXERCISE;
CALCIUM-METABOLISM; NUTRITIONAL-STATUS; FLIGHT; IGF-1
AB Bone loss and renal stone risk are longstanding concerns for astronauts. Bone resorption brought on by spaceflight elevates urinary calcium and the risk of renal stone formation. Loss of bone calcium leads to concerns about fracture risk and increased long-term risk of osteoporosis. Bone metabolism involves many factors and is interconnected with muscle metabolism and diet. We report here bone biochemistry and renal stone risk data from astronauts on 4- to 6-month International Space Station missions. All had access to a type of resistive exercise countermeasure hardware, either the Advanced Resistance Exercise Device (ARED) or the Interim Resistance Exercise Device (iRED). A subset of the ARED group also tested the bisphosphonate alendronate as a potential anti-resorptive countermeasure (Bis + ARED). While some of the basic bone marker data have been published, we provide here a more comprehensive evaluation of bone biochemistry with a larger group of astronauts. Regardless of exercise, the risk of renal stone formation increased during spaceflight. A key factor in this increase was urine volume, which was lower during flight in all groups at all time points. Thus, the easiest way to mitigate renal stone risk is to increase fluid consumption. ARED use increased bone formation without changing bone resorption, and mitigated a drop in parathyroid hormone in iRED astronauts. Sclerostin, an osteocyte-derived negative regulator of bone formation, increased 10-15% in both groups of astronauts who used the ARED (p < 0.06). IGF-1, which regulates bone growth and formation, increased during flight in all 3 groups (p < 0.001). Our results are consistent with the growing body of literature showing that the hyper-resorptive state of bone that is brought on by spaceflight can be countered pharmacologically or mitigated through an exercise-induced increase in bone formation, with nutritional support. Key questions remain about the effect of exercise-induced alterations in bone metabolism on bone strength and fracture risk. Published by Elsevier Inc.
C1 [Smith, Scott M.; Shackelford, Linda C.; Sibonga, Jean D.] NASA Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX USA.
[Heer, Martina] Univ Bonn, Dept Nutr & Food Sci, Nutr Physiol, Bonn, Germany.
[Spatz, Jordan] MIT, Beth Israel Deaconess Med Ctr, Cambridge, MA 02139 USA.
[Spatz, Jordan] MIT, Inst Med Engn & Sci, Cambridge, MA 02139 USA.
[Pietrzyk, Robert A.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Hudson, Edgar K.] JES Tech, Houston, TX USA.
[Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
RP Smith, SM (reprint author), NASA Johnson Space Ctr, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
FU NASA Human Research Program; German Aerospace Center (DLR), Germany [WB
0931]
FX The studies described here were funded by the NASA Human Research
Program, specifically the Human Health Countermeasures Element. Support
was also provided in part by grant WB 0931 from the German Aerospace
Center (DLR), Germany.
NR 47
TC 7
Z9 7
U1 0
U2 10
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 8756-3282
EI 1873-2763
J9 BONE
JI Bone
PD DEC
PY 2015
VL 81
BP 712
EP 720
DI 10.1016/j.bone.2015.10.002
PG 9
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA CX0FR
UT WOS:000365372800084
PM 26456109
ER
PT J
AU Tang, YH
Wachter, J
Rufenacht, A
FitzPatrick, GJ
Benz, SP
AF Tang, Yi-Hua
Wachter, James
Ruefenacht, Alain
FitzPatrick, Gerald J.
Benz, Samuel P.
TI Application of a 10 V Programmable Josephson Voltage Standard in Direct
Comparison With Conventional Josephson Voltage Standards
SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT
LA English
DT Article
DE Allan variance; automated comparison; Josephson arrays; Josephson
voltage standards (JVSs); uncertainty; voltage measurement
ID ALLAN VARIANCE; JUNCTIONS
AB This paper briefly describes the working principle of the 10 V programmable Josephson voltage standard (PJVS) that was developed at the National Institute of Standards and Technology and how to use it in a direct comparison with a conventional Josephson voltage standard (CJVS). Manual and automatic comparison methods were developed to verify the agreement between the two types of Josephson standards. A 10 V PJVS provided by the National Aeronautics and Space Administration (NASA) was used as a transfer standard in the 2014 Josephson voltage standard Interlaboratory Comparison that is organized by the National Conference of Standards Laboratories International. The results of automatic direct comparisons between a NASA PJVS and three CJVSs are reported. Allan variance is applied to analyze the large number of correlated data for Type A uncertainty.
C1 [Tang, Yi-Hua; FitzPatrick, Gerald J.] NIST, Gaithersburg, MD 20899 USA.
[Wachter, James] NASA, Titusville, FL 32899 USA.
[Ruefenacht, Alain; Benz, Samuel P.] NIST, Boulder, CO 80305 USA.
RP Tang, YH (reprint author), NIST, Gaithersburg, MD 20899 USA.
EM yi-hua.tang@nist.gov; james.wachter@nasa.gov; alain.rufenacht@nist.gov;
gerald.fitzpatrick@nist.gov; samuel.benz@nist.gov
NR 14
TC 1
Z9 1
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9456
EI 1557-9662
J9 IEEE T INSTRUM MEAS
JI IEEE Trans. Instrum. Meas.
PD DEC
PY 2015
VL 64
IS 12
BP 3458
EP 3466
DI 10.1109/TIM.2015.2463392
PG 9
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CW3CR
UT WOS:000364870100031
ER
PT J
AU Affolderbach, C
Du, GX
Bandi, T
Horsley, A
Treutlein, P
Mileti, G
AF Affolderbach, Christoph
Du, Guan-Xiang
Bandi, Thejesh
Horsley, Andrew
Treutlein, Philipp
Mileti, Gaetano
TI Imaging Microwave and DC Magnetic Fields in a Vapor-Cell Rb Atomic Clock
SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT
LA English
DT Article
DE Atomic clocks; diode lasers; microwave measurements; microwave
resonators; microwave spectroscopy; optical pumping
ID FREQUENCY STANDARDS; GAP RESONATOR; CAVITY; DIFFUSION; SPIN
AB We report on the experimental measurement of the dc and microwave magnetic field distributions inside a recently developed compact magnetron-type microwave cavity mounted inside the physics package of a high-performance vapor-cell atomic frequency standard. Images of the microwave field distribution with sub-100-mu m lateral spatial resolution are obtained by pulsed optical-microwave Rabi measurements, using the Rb atoms inside the cell as field probes and detecting with a CCD camera. Asymmetries observed in the microwave field images can be attributed to the precise practical realization of the cavity and the Rb vapor cell. Similar spatially resolved images of the dc magnetic field distribution are obtained by Ramsey-type measurements. The T-2 relaxation time in the Rb vapor cell is found to be position dependent and correlates with the gradient of the dc magnetic field. The presented method is highly useful for experimental in situ characterization of dc magnetic fields and resonant microwave structures, for atomic clocks or other atom-based sensors and instrumentation.
C1 [Affolderbach, Christoph; Bandi, Thejesh; Mileti, Gaetano] Univ Neuchatel, Inst Phys, Lab Temps Frequence, CH-2000 Neuchatel, Switzerland.
[Du, Guan-Xiang; Horsley, Andrew; Treutlein, Philipp] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland.
[Bandi, Thejesh] CALTECH, Jet Prop Lab, Quantum Sci & Technol Grp, Pasadena, CA 91109 USA.
RP Affolderbach, C (reprint author), Univ Neuchatel, Inst Phys, Lab Temps Frequence, CH-2000 Neuchatel, Switzerland.
EM christoph.affolderbach@unine.ch; philipp.treutlein@unibas.ch;
gaetano.mileti@unine.ch
RI Treutlein, Philipp/H-6158-2012
OI Treutlein, Philipp/0000-0001-9025-9574
FU Swiss National Science Foundation [149901, 140712, 140681]; European
Metrology Research Programme [IND55-Mclocks]; EMRP participating
countries within EURAMET; European Union
FX This work was supported in part by the Swiss National Science Foundation
under Grant 149901, Grant 140712, and Grant 140681, and in part by the
European Metrology Research Programme under Project IND55-Mclocks. The
EMRP is jointly supported by the EMRP participating countries within
EURAMET and the European Union. The Associate Editor coordinating the
review process was Dr. Sergey Kharkovsky.
NR 33
TC 2
Z9 2
U1 4
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9456
EI 1557-9662
J9 IEEE T INSTRUM MEAS
JI IEEE Trans. Instrum. Meas.
PD DEC
PY 2015
VL 64
IS 12
BP 3629
EP 3637
DI 10.1109/TIM.2015.2444261
PG 9
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CW3CR
UT WOS:000364870100047
ER
PT J
AU Van Gaest, AL
Arkoosh, MR
Dietrich, JP
AF Van Gaest, Ahna L.
Arkoosh, Mary R.
Dietrich, Joseph P.
TI Disinfection Potential of Fire Retardant Foams
SO JOURNAL OF ENVIRONMENTAL ENGINEERING
LA English
DT Article
DE Disinfection; Firefighting foams; Forest fire response; E. coli;
Coliphage
ID EARLY-LIFE STAGES; CHINOOK SALMON; ACUTE TOXICITY; MYXOBOLUS-CEREBRALIS;
QUATERNARY AMMONIUM; RAINBOW-TROUT; CHEMICALS; VIRUSES
AB The spread of aquatic invasive species during wildland firefighting activities is a concern when water sources and equipment are transported across watersheds or into pristine areas. In the present study, we investigated the capability of wildland firefighting foams to inactivate organisms in bench-scale laboratory experiments. Specifically, Escherichia coli and coliphage Phi X174 were used to test the disinfection potential of foams against bacteria and virus species as an indicator of their efficacy against more resistant organisms. The U.S. Department of Agriculture Forest Service firefighting foams tested in this study did not inactivate E. coli or coliphage during maximum exposure conditions that are feasible during firefighting activities, i.e., 10% (v:v) mix ratio and a 60-min contact time. We did not examine whether firefighting foams were effective at displacing bacterial and viral organisms when used solely as a surfactant on solid surfaces. We conclude that fire retardant foams are not effective disinfection agents and will not reduce the risk of spreading aquatic invasive viral species during firefighting activities. (C) 2015 American Society of Civil Engineers.
C1 [Van Gaest, Ahna L.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Arkoosh, Mary R.; Dietrich, Joseph P.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Dietrich, JP (reprint author), NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM vangaest@gmail.com; joseph.dietrich@noaa.gov
FU USDA Forest Service Wildland Fire Chemical Systems
FX USDA Forest Service Wildland Fire Chemical Systems for financial support
and Shirley K. Zylstra for project support.
NR 25
TC 0
Z9 0
U1 2
U2 6
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0733-9372
EI 1943-7870
J9 J ENVIRON ENG
JI J. Environ. Eng.-ASCE
PD DEC
PY 2015
VL 141
IS 12
AR 04015040
DI 10.1061/(ASCE)EE.1943-7870.0000972
PG 5
WC Engineering, Environmental; Engineering, Civil; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA CW6QQ
UT WOS:000365122800001
ER
PT J
AU Turk, FJ
Sikhakolli, R
Kirstetter, P
Durden, SL
AF Turk, F. Joseph
Sikhakolli, R.
Kirstetter, P.
Durden, S. L.
TI Exploiting Over-Land OceanSat-2 Scatterometer Observations to Capture
Short-Period Time-Integrated Precipitation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Geographic location; entity; Land surface; Atm; Ocean Structure;
Phenomena; Rainfall; Surface layer; Observational techniques and
algorithms; Microwave observations; Radars; Radar observations;
Satellite observations
ID SURFACE REFERENCE TECHNIQUE; SOIL-MOISTURE; RADAR; EMISSIVITIES;
ALGORITHMS; QUIKSCAT; RAINFALL; SENSORS; SYSTEM; US
AB Estimation of overland precipitation using observations from the radar and passive microwave radiometer sensors onboard the current Global Precipitation Measurement (GPM) and predecessor Tropical Rainfall Measuring Mission (TRMM) satellites is constrained by the underlying surface variability. The factors controlling the multichannel microwave surface emissivity and radar surface backscatter are related to surface properties such as soil type and vegetation properties that vary with location and time. Variability due to slowly varying seasonal changes can be considered when simulating radar reflectivities and radiometer equivalent blackbody brightness temperatures for use with precipitation retrieval algorithms. However, over certain surfaces, a more transient, dynamic surface change is manifested upon the onset of intermittent rain events. In these situations, a timely update of the surface state prior to each satellite overpass, together with knowledge of the associated variability in the emissivity and radar surface backscatter, may be useful to improve the performance of the overland precipitation retrieval algorithms. In this study, the potential for wide-swath surface backscatter observations from the Ku-band, dual-beam OceanSat-2 scatterometer (OSCAT) is examined as a surface reference for tracking previous-time precipitation. Over certain surfaces, it is shown that a time-change detection approach is useful to isolate the change in radar backscatter owing to previous 3-h rainfall accumulations from the more slowly varying background state. A practical use of this method would be the production of an ancillary previous-time precipitation map, which could be consulted by retrieval algorithms to select (or adjust the weighting of) candidate solutions that represent the most current surface conditions.
C1 [Turk, F. Joseph; Durden, S. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sikhakolli, R.] Indian Space Res Org, Atmospher & Ocean Sci Grp, Ahmadabad, Gujarat, India.
[Kirstetter, P.] Univ Oklahoma, Norman, OK 73019 USA.
RP Turk, FJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 300-243, Pasadena, CA 91109 USA.
EM jturk@jpl.nasa.gov
RI Kirstetter, Pierre/E-2305-2013; Measurement, Global/C-4698-2015
OI Kirstetter, Pierre/0000-0002-7381-0229;
FU NASA Precipitation Measuring Mission (PMM) science team
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. OceanSat-2 data were provided courtesy of the
Indian Space Research Organisation, and TRMM data via the NASA
Precipitation Processing System (PPS). FJT and SD acknowledge support
from the NASA Precipitation Measuring Mission (PMM) science team.
NR 39
TC 2
Z9 2
U1 1
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD DEC
PY 2015
VL 16
IS 6
BP 2519
EP 2535
DI 10.1175/JHM-D-15-0046.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CW4QD
UT WOS:000364975700008
ER
PT J
AU Johnson, JB
Kulchitsky, AV
Duvoy, P
Iagnemma, K
Senatore, C
Arvidson, RE
Moore, J
AF Johnson, Jerome B.
Kulchitsky, Anton V.
Duvoy, Paul
Iagnemma, Karl
Senatore, Carmine
Arvidson, Raymond E.
Moore, Jeffery
TI Discrete element method simulations of Mars Exploration Rover wheel
performance
SO JOURNAL OF TERRAMECHANICS
LA English
DT Article
DE Mars Exploration Rovers; Discrete element method simulation; Mobility
testing; Wheel slip
ID PARTICLE-SHAPE; MERIDIANI-PLANUM; FRICTION; CRATER; ANGLE
AB Mars Exploration Rovers (MERs) experienced mobility problems during traverses. Three-dimensional discrete element method (DEM) simulations of MER wheel mobility tests for wheel slips of i = 0, 0.1, 0.3, 0.5, 0.7, 0.9, and 0.99 were done to examine high wheel slip mobility to improve the ARTEMIS MER traverse planning tool. Simulations of wheel drawbar pull and sinkage MIT data for i 0.5 were used to determine DEM particle packing density (0.62) and contact friction (0.8) to represent the simulant used in mobility tests. The DEM simulations are in good agreement with MIT data for i = 0.5 and 0.7, with reasonable but less agreement at lower wheel slip. Three mobility stages include low slip (i < 0.3) controlled by soil strength, intermediate slip (i similar to 0.3-0.6) controlled by residual soil strength, and high slip (i similar to 0.3-0.6) controlled by residual soil strength and wheel sinkage depth. Equilibrium sinkage occurred for i < 0.9, but continuously increased for i = 0.99. Improved DEM simulation accuracy of low-slip mobility can be achieved using polyhedral particles, rather than tri-sphere particles, to represent soil. The DEM simulations of MER wheel mobility can improve ARTEMIS accuracy. (C) 2015 The Authors. Published by Elsevier Ltd. on behalf of ISTVS.
C1 [Johnson, Jerome B.; Kulchitsky, Anton V.; Duvoy, Paul] Univ Alaska Fairbanks, Inst Northern Engn, Fairbanks, AK 99775 USA.
[Iagnemma, Karl; Senatore, Carmine] MIT, Robot Mobil Grp, Lab Mfg & Prod, Cambridge, MA 02139 USA.
[Arvidson, Raymond E.] Washington Univ, St Louis, MO 63130 USA.
[Moore, Jeffery] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Johnson, JB (reprint author), Univ Alaska Fairbanks, Inst Northern Engn, POB 755910, Fairbanks, AK 99775 USA.
EM jerome.b.johnson@alaska.edu; anton.kulchitsky@alaska.edu;
pxduvoy@alaska.edu; kdi@mit.edu; senator@mit.edu;
arvidson@wunder.wustl.edu; jeff.moore@nasa.gov
FU NASA [NNX09AF54A]; Institute of Northern Engineering, University of
Alaska Fairbanks
FX This work was supported by NASA award NNX09AF54A "Physical and Geologic
Investigations of the Surface Materials along the MER Traverses:
Continuation of Co-I support to the Mars Exploration Rovers
Participating Scientist Program" and the Institute of Northern
Engineering, University of Alaska Fairbanks.
NR 37
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U1 2
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4898
EI 1879-1204
J9 J TERRAMECHANICS
JI J. Terramech.
PD DEC
PY 2015
VL 62
SI SI
BP 31
EP 40
DI 10.1016/j.jterra.2015.02.004
PG 10
WC Engineering, Environmental
SC Engineering
GA CW5RV
UT WOS:000365055200005
ER
PT J
AU Stier, B
Bednarcyk, BA
Boddeker, T
Springmann, R
Simon, JW
Reese, S
AF Stier, Bertram
Bednarcyk, Brett A.
Boeddeker, Torben
Springmann, Raphael
Simon, Jaan W.
Reese, Stefanie
TI Analysis, manufacturing, testing, and structural optimization of a novel
composite kiteboard design
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART P-JOURNAL OF
SPORTS ENGINEERING AND TECHNOLOGY
LA English
DT Article
DE Structural optimization; composite structure analysis; kiteboard design
AB A novel foam core sandwich composite kiteboard design was developed, manufactured, tested, and optimized for weight. An innovative geometry was developed to improve performance under the demanding operating conditions experienced by waterborne kiteboards. A computer-aided design model was built and used to produce a tool, which was used in the construction of a prototype kiteboard. The prototype was tested under three-point bend loading, with full-field strain measurements recorded during the test. Both shell and solid finite element models of the kiteboard were developed and validated via comparison with the test data, where the composite material properties used in the models were obtained via coupon tests. The validated shell finite element model was then used in conjunction with the HyperSizer aerospace composite design software to optimize the kiteboard design for minimum weight, while also checking a wide array of composite and sandwich panel failure criteria.
C1 [Stier, Bertram; Boeddeker, Torben; Springmann, Raphael; Simon, Jaan W.; Reese, Stefanie] Rhein Westfal TH Aachen, Inst Appl Mech IFAM, Aachen, Germany.
[Bednarcyk, Brett A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Bednarcyk, BA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 49-7, Cleveland, OH 44135 USA.
EM Brett.A.Bednarcyk@nasa.gov
RI Simon, Jaan/J-9114-2014
OI Simon, Jaan/0000-0003-2231-2569
FU Deutsche Forschungsgemeinschaft (DFG); Daimler und Benz Stiftung
FX The study was financially supported by the Deutsche
Forschungsgemeinschaft (DFG) and the Daimler und Benz Stiftung. The
authors also thank Collier Research Corp. for providing the HyperSizer
software and Jeff Smith of South Coast Custom Surfboards (Bournemouth,
UK) for providing the photographs shown in Figure 2.
NR 19
TC 0
Z9 0
U1 0
U2 1
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1754-3371
EI 1754-338X
J9 P I MECH ENG P-J SPO
JI Proc. Inst. Mech. Eng. Part P-J. Sport. Eng. Technol.
PD DEC
PY 2015
VL 229
IS 4
BP 248
EP 265
DI 10.1177/1754337115584874
PG 18
WC Engineering, Mechanical; Sport Sciences
SC Engineering; Sport Sciences
GA CW8MZ
UT WOS:000365255100005
ER
PT J
AU Arisman, CJ
Johansen, CT
Bathel, BF
Danehy, PM
AF Arisman, C. J.
Johansen, C. T.
Bathel, B. F.
Danehy, P. M.
TI Investigation of Gas Seeding for Planar Laser-Induced Fluorescence in
Hypersonic Boundary Layers
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 50th AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 06-13, 2012
CL Nashville, TN
SP AIAA, US AF Off Sci Res
ID ESSENTIALLY NONOSCILLATORY SCHEMES; CONSERVATION-LAWS; SKIN-FRICTION;
FLOWS; TRANSITION; EQUATIONS; VISUALIZATION; COMBUSTION; HYDROGEN
AB Numerical simulations of the gas-seeding strategies required for planar laser-induced fluorescence in a Mach 10 (approximately Mach 8.2 postshock) airflow were performed. The work was performed to understand and quantify the adverse effects associated with gas seeding and to assess various types of seed gas that could potentially be used in future experiments. In prior experiments, NO and NO2 were injected through a slot near the leading edge of a flatplate wedge model used in NASA Langley Research Center's 31 in. Mach 10 air tunnel facility. In this paper, nitric oxide, krypton, and iodine gases were simulated at various injection rates. Simulations showing the deflection of the velocity boundary layer for each of the cases are presented. Streamwise distributions of velocity and concentration boundary-layer thicknesses, as well as vertical distributions of velocity, temperature, and mass distributions, are presented for each of the cases. A comparison between simulated streamwise velocity profiles and experimentally obtained molecular tagging velocimetry profiles using a nitric oxide seeding strategy is performed to verify the influence of such a strategy on the boundary layer. The relative merits of the different seeding strategies are discussed. The results from a custom solver based on OpenFOAM version 2.2.1 are compared against results obtained from ANSYS (R) Fluent version 6.3.
C1 [Arisman, C. J.; Johansen, C. T.] Univ Calgary, Dept Mech & Mfg Engn, Calgary, AB T2N 1N4, Canada.
[Bathel, B. F.; Danehy, P. M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
RP Arisman, CJ (reprint author), Univ Calgary, Dept Mech & Mfg Engn, Calgary, AB T2N 1N4, Canada.
NR 50
TC 5
Z9 5
U1 1
U2 14
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD DEC
PY 2015
VL 53
IS 12
BP 3637
EP 3651
DI 10.2514/1.J053892
PG 15
WC Engineering, Aerospace
SC Engineering
GA CW6MV
UT WOS:000365112500010
ER
PT J
AU Tokugawa, N
Choudhari, M
Ishikawa, H
Ueda, Y
Fujii, K
Atobe, T
Li, F
Chang, CL
White, J
AF Tokugawa, Naoko
Choudhari, Meelan
Ishikawa, Hiroaki
Ueda, Yoshine
Fujii, Keisuke
Atobe, Takashi
Li, Fei
Chang, Chau-Lyan
White, Jeffery
TI Pressure Gradient Effects on Supersonic Transition over Axisymmetric
Bodies at Incidence
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Fluid Dynamics Conference and Exhibit
CY JUN 25-28, 2012
CL New Orleans, LA
SP AIAA
ID BOUNDARY-LAYER-TRANSITION; CONE; MACH-3.5
AB Boundary-layer transition on axisymmetric bodies at a nonzero angle of attack in Mach 2 supersonic flow was investigated using experimental measurements and linear stability analysis. Transition over four axisymmetric bodies (namely, the Sears-Haack body, the semi-Sears-Haack body, the straight cone, and the flared cone) with different axial pressure gradients was measured in two different facilities with different unit Reynolds numbers. The semi-Sears-Haack body and flared cone were designed specifically to achieve a broader range of axial pressure distributions. Measurements revealed a dramatic effect of body shape on transition behavior near the leeward plane of symmetry. For a body shape with an adverse pressure gradient (that is, a flared cone), the measured transition patterns show an earlier transition location along the leeward symmetry plane in comparison with the neighboring azimuthal locations. For a nearly zero pressure gradient (that is, the straight cone), such leeward-first transition is observed only at the larger unit Reynolds number. Finally, transition occurs farther downstream along the leeward plane for the remaining two body shapes with a favorable pressure gradient. The observed transition patterns are partially consistent with the numerical predictions based on linear stability analysis.
C1 [Tokugawa, Naoko] Japan Aerosp Explorat Agcy, Aeronaut Technol Directorate, Tokyo 1810015, Japan.
[Choudhari, Meelan; Li, Fei; Chang, Chau-Lyan; White, Jeffery] NASA, Langley Res Ctr, Computat Aero Sci Branch, Hampton, VA 23681 USA.
[Ishikawa, Hiroaki] ASIRI Inc, Tokyo 1631343, Japan.
[Ueda, Yoshine] Tryangle Inc, Tokyo 1600023, Japan.
[Fujii, Keisuke; Atobe, Takashi] Japan Aerosp Explorat Agcy, Aeronaut Technol Directorate, Chofu, Tokyo 1828522, Japan.
RP Tokugawa, N (reprint author), Japan Aerosp Explorat Agcy, Aeronaut Technol Directorate, Tokyo 1810015, Japan.
EM tokugawa.naoko@jaxa.jp
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
NR 24
TC 1
Z9 1
U1 0
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD DEC
PY 2015
VL 53
IS 12
BP 3737
EP 3751
DI 10.2514/1.J054070
PG 15
WC Engineering, Aerospace
SC Engineering
GA CW6MV
UT WOS:000365112500018
ER
PT J
AU Stanford, BK
AF Stanford, Bret K.
TI Role of Unsteady Aerodynamics During Aeroelastic Optimization
SO AIAA JOURNAL
LA English
DT Editorial Material
ID DOUBLET-LATTICE METHOD; STRUCTURAL OPTIMIZATION; CONSTRAINTS
C1 [Stanford, Bret K.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Stanford, BK (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
EM bret.k.stanford@nasa.gov
NR 13
TC 0
Z9 0
U1 3
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD DEC
PY 2015
VL 53
IS 12
BP 3826
EP 3831
DI 10.2514/1.J054314
PG 6
WC Engineering, Aerospace
SC Engineering
GA CW6MV
UT WOS:000365112500025
ER
PT J
AU McElroy, M
Leone, F
Ratcliffe, J
Czabaj, M
Yuan, FG
AF McElroy, M.
Leone, F.
Ratcliffe, J.
Czabaj, M.
Yuan, F. G.
TI Simulation of delamination-migration and core crushing in a CFRP
sandwich structure
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Laminates; Honeycomb; Damage mechanics; Delamination
ID LOW-VELOCITY IMPACT; LAMINATED COMPOSITES; HONEYCOMB CORE; SUBSEQUENT
MIGRATION; DAMAGE; BEHAVIOR; GROWTH; MODEL; COMPRESSION; FRACTURE
AB Following the onset of damage caused by an impact load on a composite laminate structure, delaminations often form propagating outwards from the point of impact and in some cases can migrate via matrix cracks between plies as they grow. The goal of the present study is to develop an accurate finite element modeling technique for simulation of the delamination migration phenomena in laminate impact damage processes. An experiment was devised where, under a quasi-static indentation load, an embedded delamination in the facesheet of a laminate sandwich specimen migrates via a transverse matrix crack and then continues to grow on a new ply interface. Using data from this test for validation purposes, several finite element damage simulation methods were investigated. Comparing the experimental results with those of the different models reveals certain modeling features that are important to include in a numerical simulation of delamination migration and some that may be neglected. Published by Elsevier Ltd.
C1 [McElroy, M.; Ratcliffe, J.] NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Hampton, VA 23665 USA.
[Leone, F.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23665 USA.
[McElroy, M.; Yuan, F. G.] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA.
[Czabaj, M.] Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA.
RP McElroy, M (reprint author), 2 W Reid St,Mail Stop 188E, Hampton, VA 23681 USA.
EM mark.w.mcelroy@nasa.gov
NR 39
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U1 2
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
EI 1878-5840
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD DEC
PY 2015
VL 79
BP 192
EP 202
DI 10.1016/j.compositesa.2015.08.026
PG 11
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA CW3MG
UT WOS:000364895800021
ER
PT J
AU Desai, S
Wahr, J
Beckley, B
AF Desai, Shailen
Wahr, John
Beckley, Brian
TI Revisiting the pole tide for and from satellite altimetry
SO JOURNAL OF GEODESY
LA English
DT Article
DE Pole tide; Satellite altimetry; Chandler wobble; Geocenter motion; Load
tide
ID SEA-LEVEL; OCEAN TIDES; NORTH-SEA; CHANDLER-WOBBLE; TIME-SERIES;
TOPEX/POSEIDON; DEFORMATION; JASON-1; MISSION; EARTH
AB Satellite altimeter sea surface height observations include the geocentric displacements caused by the pole tide, namely the response of the solid Earth and oceans to polar motion. Most users of these data remove these effects using a model that was developed more than 20 years ago. We describe two improvements to the pole tide model for satellite altimeter measurements. Firstly, we recommend an approach that improves the model for the response of the oceans by including the effects of self-gravitation, loading, and mass conservation. Our recommended approach also specifically includes the previously ignored displacement of the solid Earth due to the load of the ocean response, and includes the effects of geocenter motion. Altogether, this improvement amplifies the modeled geocentric pole tide by 15 %, or up to 2 mm of sea surface height displacement. We validate this improvement using two decades of satellite altimeter measurements. Secondly, we recommend that the altimetry pole tide model exclude geocentric sea surface displacements resulting from the long-term drift in polar motion. The response to this particular component of polar motion requires a more rigorous approach than is used by conventional models. We show that erroneously including the response to this component of polar motion in the pole tide model impacts interpretation of regional sea level rise by 0.25 mm/year.
C1 [Desai, Shailen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Wahr, John] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Beckley, Brian] SGT Inc, Greenbelt, MD USA.
RP Desai, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA.
EM Shailen.Desai@jpl.nasa.gov
FU NASA
FX SDD performed the work described in this paper at the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
National Aeronautics and Space Administration. Work at the University of
Colorado was partially supported by NASA GRACE funding, and by NASA's
'Making Earth Science Data Records for Use in Research Environments
(MEaSUREs) Program. We thank G. Egbert and S. Erofeeva for providing the
TPXO8 ocean tide model. The IERS is acknowledged for providing the
EOPC04 polar motion time series. We thank two anonymous reviewers for
their useful feedback.
NR 40
TC 1
Z9 1
U1 2
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
EI 1432-1394
J9 J GEODESY
JI J. Geodesy
PD DEC
PY 2015
VL 89
IS 12
BP 1233
EP 1243
DI 10.1007/s00190-015-0848-7
PG 11
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA CW3TW
UT WOS:000364915800006
ER
PT J
AU Nikolic, D
Madzunkov, SM
Darrach, MR
AF Nikolic, Dragan
Madzunkov, Stojan M.
Darrach, Murray R.
TI Computer Modeling of an Ion Trap Mass Analyzer, Part I: Low Pressure
Regime
SO JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY
LA English
DT Article
DE Quadrupole ion trap; Mass spectrometry; Charged particle manipulation
ID RESONANCE EXCITATION; MULTIPARTICLE SIMULATION; SPECTROMETER;
TRAJECTORIES; DYNAMICS; INJECTION; EJECTION; SIMION; MOTION; DC
AB We present the multi-particle simulation program suite Computational Ion Trap Analyzer (CITA) designed to calculate the ion trajectories within a Paul quadrupole ion trap developed by the Jet Propulsion Laboratory (JPL). CITA uses an analytical expression of the electrodynamic field, employing up to six terms in multipole expansion and a modified velocity-Verlet method to numerically calculate ion trajectories. The computer code is multithreaded and designed to run on shared-memory architectures. CITA yields near real-time simulations with full propagation of 26 particles per second per core. As a consequence, a realistic numbers of trapped ions (100+ million) can be used and their trajectories modeled, yielding a representative prediction of mass spectrometer analysis of trace gas species. When the model is compared with experimental results conducted at low pressures using the conventional quadrupole and dipole excitation modes, there is an excellent agreement with the observed peak shapes. Owing to the program's efficiency, CITA has been used to explore regions of trapping stability that are of interest to experimental research. These results are expected to facilitate a fast and reliable modeling of ion dynamics in miniature quadrupole ion trap and improve the interpretation of observed mass spectra.
C1 [Nikolic, Dragan; Madzunkov, Stojan M.; Darrach, Murray R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nikolic, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dragan.nikolic@jpl.nasa.gov
FU JPL's Research and Technology Development Program; California Institute
of Technology; U.S. Government
FX The authors acknowledge that this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. It was
supported by the JPL's Research and Technology Development Program. The
authors also acknowledge the valuable contributions of Jurij Simcic
(JPL) in the design and detailed engineering of 3D models used in this
study. Copyright 2015 California Institute of Technology; U.S.
Government sponsorship is acknowledged.
NR 38
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U1 5
U2 14
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1044-0305
EI 1879-1123
J9 J AM SOC MASS SPECTR
JI J. Am. Soc. Mass Spectrom.
PD DEC
PY 2015
VL 26
IS 12
BP 2115
EP 2124
DI 10.1007/s13361-015-1236-5
PG 10
WC Biochemical Research Methods; Chemistry, Analytical; Chemistry,
Physical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA CW6OI
UT WOS:000365116500017
PM 26286456
ER
PT J
AU Wulder, MA
Hilker, T
White, JC
Coops, NC
Masek, JG
Pflugmacher, D
Crevier, Y
AF Wulder, Michael A.
Hilker, Thomas
White, Joanne C.
Coops, Nicholas C.
Masek, Jeffrey G.
Pflugmacher, Dirk
Crevier, Yves
TI Virtual constellations for global terrestrial monitoring
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Satellite; Constellation; Monitoring; Land cover; Land use; Science;
Landsat; Sentinel-2
ID LAND-COVER CHANGE; REMOTELY-SENSED DATA; EARTH OBSERVATION REQUIREMENTS;
RESOLUTION SATELLITE IMAGERY; FOREST CANOPY HEIGHT; ABOVEGROUND BIOMASS;
CLIMATE-CHANGE; TIME-SERIES; SPATIAL-RESOLUTION; SURFACE REFLECTANCE
AB Free and open access to satellite imagery and value-added data products have revolutionized the role of remote sensing in Earth system science. Nonetheless, rapid changes in the global environment pose challenges to the science community that are increasingly difficult to address using data from single satellite sensors or platforms due to the underlying limitations of data availability and tradeoffs that govern the design and implementation of currently existing sensors. Virtual constellations of planned and existing satellite sensors may help to overcome this limitation by combining existing observations to mitigate limitations of any one particular sensor. While multi-sensor applications are not new, the integration and harmonization of multi-sensor data is still challenging, requiring tremendous efforts of science and operational user communities.
Defined by the Committee on Earth Observation Satellites (CEOS) as a "set of space and ground segment capabilities that operate in a coordinated manner to meet a combined and common set of Earth Observation requirements", virtual constellations can principally be used to combine sensors with similar spatial, spectral, temporal, and radiometric characteristics. We extend this definition to also include sensors that are principally incompatible, because they are fundamentally different (for instance active versus passive remote sensing systems), but their combination is necessary and beneficial to achieve a specific monitoring goal. In this case, constellations are more likely to build upon the complementarity of resultant information products from these incompatible sensors rather than the raw physical measurements. In this communication, we explore the potential and possible limitations to be overcome regarding virtual constellations for terrestrial science applications, discuss potentials and limitations of various candidate sensors, and provide context on integration of sensors. Thematically, we focus on land-cover and land-use change (LCLUC), with emphasis given to medium spatial resolution (Le., pixels sided 10 to 100 m) sensors, specifically as a complement to those onboard the Landsat series of satellites. We conclude that virtual constellations have the potential to notably improve observation capacity and thereby Earth science and monitoring programs in general. Various national and international parties have made notable and valuable progress related to virtual constellations. There is, however, inertia inherent to Earth observation programs, largely related to their complexity, as well as national interests, observation aims, and high system costs. Herein we define and describe virtual constellations, offer the science and applications information needs to offer context, provide the scientific support for a range of virtual constellation levels based upon applications readiness, capped by a discussion of issues and opportunities toward facilitating implementation of virtual constellations (in their various forms). Crown Copyright (C) 2015 Published by Elsevier Inc All rights reserved.
C1 [Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
[Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Coops, Nicholas C.] Univ British Columbia, Forest Sci Ctr, Dept Forest Resource Management, Vancouver, BC V6T 1Z4, Canada.
[Masek, Jeffrey G.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pflugmacher, Dirk] Humboldt Univ, Dept Geog, D-10099 Berlin, Germany.
[Crevier, Yves] Canadian Space Agcy, Earth Observat Applicat & Utilizat, Space Utilizat Directorate, St Hubert, PQ J3Y 8Y9, Canada.
RP Wulder, MA (reprint author), Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, 506 West Burnside Rd, Victoria, BC V8Z 1M5, Canada.
EM mike.wulder@canada.ca
RI Masek, Jeffrey/D-7673-2012; Coops, Nicholas/J-1543-2012; Wulder,
Michael/J-5597-2016
OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896
FU Canadian Space Agency (CSA) Government Related Initiatives Program
(GRIP); Canadian Forest Service (CFS) of Natural Resources Canada
FX This research was undertaken as part of the "National Terrestrial
Ecosystem Monitoring System (NTEMS): Timely and detailed national
cross-sector monitoring for Canada" project jointly funded by the
Canadian Space Agency (CSA) Government Related Initiatives Program
(GRIP) and the Canadian Forest Service (CFS) of Natural Resources
Canada. Deliberations of the Landsat Science Team have also informed
this material. The editor and reviewers are thanked for their
constructive and insightful reviews and suggestions to improve this
manuscript.
NR 145
TC 12
Z9 13
U1 5
U2 27
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2015
VL 170
BP 62
EP 76
DI 10.1016/j.rse.2015.09.001
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CW1CB
UT WOS:000364726100006
ER
PT J
AU Zimmerman, M
Oddy, D
Stolen, E
Breininger, D
Pruett, CL
AF Zimmerman, Monica
Oddy, Donna
Stolen, Eric
Breininger, David
Pruett, Christin L.
TI Microspatial sampling reveals cryptic influences on gene flow in a
threatened mammal
SO CONSERVATION GENETICS
LA English
DT Article
DE Approximate Bayesian computation; Landscape genetics; Movement barrier;
Microsatellite; Peromyscus polionotus niveiventris
ID PEROMYSCUS-POLIONOTUS-NIVEIVENTRIS; APPROXIMATE BAYESIAN COMPUTATION;
POLYMORPHIC MICROSATELLITE MARKERS; CORRELATED ALLELE FREQUENCIES;
MULTILOCUS GENOTYPE DATA; POPULATION-GENETICS; BEACH MOUSE; HABITAT
OCCUPANCY; SOFTWARE; DNA
AB We studied the population structure and historical demography of the last remaining core population of the threatened southeastern beach mouse (SEBM; Peromyscus polionotus niveiventris) located on a federally protected barrier island complex at the Kennedy Space Center (KSC), Merritt Island National Wildlife Refuge (MINWR) and Cape Canaveral Air Force Station (CCAFS) in Florida, USA. Beach mice (N = 171) were collected from 33 trapping locations along 30 km of coastline on KSC/MINWR/CCAFS and were genotyped using 10 microsatellite loci. We found four genetic clusters of mice that likely form a metapopulation. Gene flow among clusters, assessed using assignment tests, was limited suggesting that human development can serve to inhibit dispersal of beach mice. However, when the presence of roads were examined as possible barriers to movement, gene flow appeared to be facilitated suggesting that removal of thick vegetation along roadsides increases movement. We used approximate Bayesian computation (ABC) to estimate divergence time among clusters and effective population sizes for each cluster and for the pre-divergence population. Results of ABC analyses suggest that barriers to movement likely formed following the construction of the John F. Kennedy Space Center beginning in the 1960s but that this has not heavily impacted the effective size of populations. Pre-divergence and contemporary effective sizes are similar, thus, population sizes likely remained relatively large over the last 50-100 years. The population of SEBM on KSC/MINWR/CCAFS appears to be a genetically diverse core population and individuals from this population will most likely be good candidates for any future reintroduction and translocation programs.
C1 [Zimmerman, Monica; Pruett, Christin L.] Florida Inst Technol, Dept Biol, Melbourne, FL 32901 USA.
[Oddy, Donna; Stolen, Eric; Breininger, David] NASA, Ecol Programs, InoMed Hlth Applicat, Kennedy Space Ctr, FL 32899 USA.
RP Pruett, CL (reprint author), Florida Inst Technol, Dept Biol, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM cpruett@fit.edu
FU NASA; Florida Institute of Technology
FX We thank NASA and Florida Institute of Technology for funding this
research. We thank C. Hall and L. Phillips for aid in logistics and S.
Gann, S. Legare, K. Holloway-Adkins, S. Weiss, S. Sneckenberger, and S.
Trapp for tissue collection. We also thank M. Bush and J. Trefry for
comments on an early version of this manuscript.
NR 62
TC 0
Z9 0
U1 3
U2 27
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1566-0621
EI 1572-9737
J9 CONSERV GENET
JI Conserv. Genet.
PD DEC
PY 2015
VL 16
IS 6
BP 1403
EP 1414
DI 10.1007/s10592-015-0749-6
PG 12
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA CV0QZ
UT WOS:000363957700011
ER
PT J
AU Sturdivant, SK
Perchik, M
Brill, RW
Bushnell, PG
AF Sturdivant, S. Kersey
Perchik, Marieke
Brill, Richard W.
Bushnell, Peter G.
TI Metabolic responses of the Nereid polychaete, Alitta succinea, to
hypoxia at two different temperatures
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Stopflow respirometry; Oxyregulation; Oxygen; Critical saturation;
Benthic function
ID OXYGEN-UPTAKE; ANAEROBIC METABOLISM; SEDIMENTS; BIOTURBATION;
ECOSYSTEMS; VENTILATION; ADAPTATIONS; CALIFORNIA; ORGANISMS; COMMUNITY
AB Coastal hypoxia has detrimental effects to community ecology, degrading community structure and diminishing benthic function. Benthic function is largely driven by infauna bioturbation, which facilitates life-supporting processes by increasing the quality of marine sediments for nearly all biota. These infauna-mediated processes are diminished by coastal hypoxia. However, some infauna have been documented to exhibit metabolic plasticity to low oxygen allowing them to maintain some form of benthic function. Of particular interest to this study is the Nereid polychaete Alitta succinea. Stopflow respirometry was used to assess the hypoxic tolerance of A. succinea, by quantifying resting metabolic rate (V-O2), critical oxygen saturation (i.e. the oxygen level below which worms could not maintain aerobic metabolism), and the oxyregulation ability at an acclimation temperature (25 degrees C) and after an acute temperature increase (to 30 degrees C). The acute Q(10) during normoxia was 4.6, though this effect of temperature on V-O2, was completely muted during hypoxia with a Q(10) of 1. Compared among other polychaetes, A. succinea was the most efficient at oxyregulation, resulting in low critical oxygen saturation levels of 16% and 10% at 25 and 30 degrees C, respectively. Finally, there was a significant effect of hypoxia on the mass metabolism relationship of A. succinea. Oxygen consumption rates were significantly higher during hypoxia only for smaller A. succinea, suggesting a physiological size selection for hypoxia response. These findings demonstrate the significant effect of hypoxia on A. succinea metabolism, but also provide the metabolic justification for survival of this infaunal worm during severe hypoxia. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Sturdivant, S. Kersey] Duke Univ, Nicholas Sch Environm, Div Marine Sci & Conservat, Beaufort, NC 28516 USA.
[Sturdivant, S. Kersey] INSPIRE Environm, Newport, RI 02840 USA.
[Perchik, Marieke] Allegheny Coll, Dept Environm Sci, Meadville, PA 16335 USA.
[Brill, Richard W.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA.
[Brill, Richard W.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, Highlands, NJ 07732 USA.
[Bushnell, Peter G.] Indiana Univ, Dept Biol Sci, South Bend, IN 46634 USA.
RP Sturdivant, SK (reprint author), Duke Univ, Nicholas Sch Environm, Div Marine Sci & Conservat, 135 Duke Marine Lab Rd, Beaufort, NC 28516 USA.
EM kersey@inspireenvironmental.com
FU NSF; Duke University Marine Lab
FX Supported in part by NSF funded OCE-PRF and Duke University Marine Lab
funded Joseph S. Ramus Endowment to S.K.S. We also thank D. Forward for
a helpful critique and critical discussions. [SS]
NR 83
TC 3
Z9 3
U1 3
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD DEC
PY 2015
VL 473
BP 161
EP 168
DI 10.1016/j.jembe.2015.09.001
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA CV4TI
UT WOS:000364259000019
ER
EF