FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Loaiza, J
Gutierrez, L
Correa, M
Bermingham, E
Scott, M
Wilkerson, R
Birnberg, L
Grijalva, M
Rovira, J
Bickersmith, S
Conn, JE
AF Loaiza, Jose
Gutierrez, Lina
Correa, Margarita
Bermingham, Eldredge
Scott, Marilyn
Wilkerson, Richard
Birnberg, Lotty
Grijalva, Mario
Rovira, Jose
Bickersmith, Sara
Conn, Jan E.
TI PLEISTOCENE GEOGRAPHIC SEPARATION IN EASTERN PANAMA AND NORTHERN
COLOMBIA LEADS TO POPULATION STRUCTURE IN ANOPHELES (NYSSORHYNCHUS)
ALBIMANUS (DIPTERA: CULICIDAE)
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Meeting Abstract
CT 58th Annual Meeting of the
American-Society-of-Tropical-Medicine-and-Hygiene
CY NOV 18-22, 2009
CL Washington, DC
SP Amer Soc Trop Med & Hyg
C1 [Loaiza, Jose; Scott, Marilyn] McGill Univ, Montreal, PQ 20560, Canada.
[Gutierrez, Lina; Correa, Margarita] Univ Antioquia, Escuela Microbiol, Medellin, Colombia.
[Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, 45701, Panama.
[Wilkerson, Richard] Smithsonian Inst, Walter Reed Army Inst Res, Washington, DC USA.
[Birnberg, Lotty] Pontif Catholic Univ Ecuador, Ctr Infect Dis Res, Quito, Ecuador.
[Grijalva, Mario] Ohio Univ, Trop Dis Inst, Athens, OH USA.
[Rovira, Jose] Inst Conmemorat Gorgas Estudios Salud, Panama City, Panama.
[Bickersmith, Sara; Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD NOV
PY 2009
VL 81
IS 5
SU S
MA 718
BP 206
EP 207
PG 2
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 521WK
UT WOS:000271956701134
ER
PT J
AU Leirana, MM
Harlow, W
Hildebrandt, J
Silva-do-Nascimento, TF
Lourenco-de-Oliveira, R
Sallum, MAM
Fritz, GN
Ruiz, F
Wilkerson, R
Loaiza, JR
Dantur, MJ
Povoa, MAM
Gutierrez-Builes, LA
Correa, MO
Conn, JE
AF Leirana, Marta Moreno
Harlow, Wesley
Hildebrandt, Jessica
Fernandes Silva-do-Nascimento, Teresa
Lourenco-de-Oliveira, Ricardo
Mureb Sallum, Maria Anice
Fritz, Gary N.
Ruiz, Freddy
Wilkerson, Richard
Loaiza, Jose R.
Julia Dantur, Maria
Povoa, Marinete A. M.
Andrea Gutierrez-Builes, Lina
Correa, Margarita O.
Conn, Jan E.
TI NEOTROPICAL ANOPHELES TRIANNULATUS COMPLEX: PHYLOGEOGRAPHY AND
DEMOGRAPHIC HISTORY BASED ON MITOCHONDRIAL AND NUCLEAR MARKERS
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Meeting Abstract
CT 58th Annual Meeting of the
American-Society-of-Tropical-Medicine-and-Hygiene
CY NOV 18-22, 2009
CL Washington, DC
SP Amer Soc Trop Med & Hyg
C1 [Leirana, Marta Moreno; Harlow, Wesley; Hildebrandt, Jessica; Conn, Jan E.] New York Dept Hlth, Wadsworth Ctr, Albany, NY USA.
[Fernandes Silva-do-Nascimento, Teresa; Lourenco-de-Oliveira, Ricardo] Inst Oswaldo Cruz Fiocruz, Dept Entomol, Rio De Janeiro, Brazil.
[Mureb Sallum, Maria Anice] Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, Brazil.
[Fritz, Gary N.] Eastern Illinois Univ, Dept Biol Sci, Charleston, IL 61920 USA.
[Ruiz, Freddy; Wilkerson, Richard] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD USA.
[Loaiza, Jose R.] Smithsonian Trop Res Inst, Balboa, Panama.
[Julia Dantur, Maria] Univ Nacl Tucuman, Inst Super Entomol Dr Abraham Willink, Fac Ciencias, Nat & Inst Miguel Lillo, San Miguel De Tucuman, Argentina.
[Povoa, Marinete A. M.] Inst Evandro Chagas, Seccao Parasitol, Belem, Para, Brazil.
[Andrea Gutierrez-Builes, Lina; Correa, Margarita O.] Univ Antioquia, Grp Microbiol Mol, Escuela Microbiol, Medellin, Colombia.
RI Sallum, Maria/B-8537-2012
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD NOV
PY 2009
VL 81
IS 5
SU S
MA 722
BP 208
EP 208
PG 1
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 521WK
UT WOS:000271956701138
ER
PT J
AU McKeon, SN
Lehr, MA
Kilpatrick, CW
Wilkerson, RC
Salum, MA
Pereira, JB
Conn, JE
AF McKeon, S. N.
Lehr, M. A.
Kilpatrick, C. W.
Wilkerson, R. C.
Salum, M. A.
Pereira, J. B.
Conn, J. E.
TI PHYLOGENETIC RELATIONSHIP AND POPULATION STRUCTURE OF THE NEOTROPICAL
MALARIA VECTOR ANOPHELES MARAJOARA (DIPTERA: CULICIDAE) USING MULTIPLE
MOLECULAR MARKERS
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Meeting Abstract
CT 58th Annual Meeting of the
American-Society-of-Tropical-Medicine-and-Hygiene
CY NOV 18-22, 2009
CL Washington, DC
SP Amer Soc Trop Med & Hyg
C1 [McKeon, S. N.] SUNY Albany, Sch Publ Hlth, Slingerlands, NY USA.
[Lehr, M. A.; Kilpatrick, C. W.] Univ Vermont, Coll Arts & Sci, Burlington, VT USA.
[Wilkerson, R. C.] Smithsonian Inst, Walter Reed Army Inst Res, Washington, DC 20560 USA.
[Salum, M. A.] Univ Sao Paulo, Fac Saude Publ, Sao Paulo, Brazil.
[Pereira, J. B.] Inst Oswaldo Cruz, Lab Fisiol & Controle Artropodes Vetores, BR-20001 Rio De Janeiro, Brazil.
[Conn, J. E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Albany, NY USA.
NR 0
TC 0
Z9 0
U1 1
U2 3
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD NOV
PY 2009
VL 81
IS 5
SU S
MA 963
BP 277
EP 278
PG 2
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 521WK
UT WOS:000271956701377
ER
PT J
AU Wilkerson, RC
Spindler, V
Sallum, MA
Povoa, MM
Correa, MM
Gutierrez, LA
Rangel, Y
Conn, JE
AF Wilkerson, Richard C.
Spindler, Victoria
Sallum, Maria Anice
Povoa, Marinete M.
Correa, Margarita M.
Gutierrez, Lina A.
Rangel, Yadira
Conn, Jan E.
TI LINEAGE DIVERGENCE IN THE NEOTROPICAL MALARIA VECTOR ANOPHELES
(NYSSORHYNCHUS) NUNEZTOVARI AND ITS SISTER TAXON AN. GOELDII (DIPTERA:
CULICIDAE) BASED ON NUCLEAR WHITE AND MTDNA COI SEQUENCE ANALYSIS
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Meeting Abstract
CT 58th Annual Meeting of the
American-Society-of-Tropical-Medicine-and-Hygiene
CY NOV 18-22, 2009
CL Washington, DC
SP Amer Soc Trop Med & Hyg
C1 [Wilkerson, Richard C.] Smithsonian Inst, Walter Reed Army Inst Res, Washington, DC 20560 USA.
[Spindler, Victoria] SUNY Albany, Sch Publ Hlth, Albany, NY USA.
[Sallum, Maria Anice] Univ Sao Paulo, Fac Saude Publ, Sao Paulo, Brazil.
[Povoa, Marinete M.] Inst Evandro Chagas, Programa Pesquisas Malaria, Belem, Para, Brazil.
[Correa, Margarita M.; Gutierrez, Lina A.] Univ Antioquia, Escuela Microbiol, Medellin, Colombia.
[Rangel, Yadira] Cent Univ Venezuela, Inst Zool Trop, Caracas, Venezuela.
[Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA.
RI Sallum, Maria/B-8537-2012
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD NOV
PY 2009
VL 81
IS 5
SU S
MA 965
BP 278
EP 278
PG 1
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 521WK
UT WOS:000271956701379
ER
PT J
AU Kilpatrick, AM
Peters, RJ
Jones, MJ
Marra, PP
Daszak, P
Kramer, LD
AF Kilpatrick, A. Marm
Peters, Ryan J.
Jones, Matthew J.
Marra, Peter P.
Daszak, Peter
Kramer, Laura D.
TI VACCINATION OF WILDLIFE TO CONTROL ZOONOTIC DISEASE: WEST NILE VIRUS AS
A CASE STUDY
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Meeting Abstract
CT 58th Annual Meeting of the
American-Society-of-Tropical-Medicine-and-Hygiene
CY NOV 18-22, 2009
CL Washington, DC
SP Amer Soc Trop Med & Hyg
C1 [Kilpatrick, A. Marm] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Peters, Ryan J.] George Mason Univ, Fairfax, VA 22030 USA.
[Jones, Matthew J.; Kramer, Laura D.] New York State Dept Hlth, Albany, NY USA.
[Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC USA.
[Daszak, Peter] Wildlife Trust, New York, NY USA.
NR 0
TC 1
Z9 1
U1 0
U2 4
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD NOV
PY 2009
VL 81
IS 5
SU S
MA 1100
BP 318
EP 318
PG 1
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 521WK
UT WOS:000271956701514
ER
PT J
AU Smith, AR
Kapheim, KM
O'Donnell, S
Wcislo, WT
AF Smith, Adam R.
Kapheim, Karen M.
O'Donnell, Sean
Wcislo, William T.
TI Social competition but not subfertility leads to a division of labour in
the facultatively social sweat bee Megalopta genalis (Hymenoptera:
Halictidae)
SO ANIMAL BEHAVIOUR
LA English
DT Article
DE body size; division of labour; evolution of eusociality; Megalopta
genalis; queen removal; social competition; social flexibility;
subfertility; sweat bee
ID PRIMITIVELY EUSOCIAL BEE; BODY-SIZE; ECUADORIA HYMENOPTERA; ZEPHYRUM
HYMENOPTERA; CASTE DETERMINATION; POLISTES-GALLICUS; BOMBUS-TERRESTRIS;
SOLITARY BEE; EVOLUTION; WASP
AB Insects with facultative social behaviour permit direct examination of factors associated with the expression of division of labour: why do some females remain in their natal nest as nonreproductive foragers, while others disperse? The facultatively social halictid bee Megalopta genalis shows strong reproductive division of labour, associated with body size ( foragers tend to be smaller than queens and dispersers). We used M. genalis to test two hypotheses for the expression of worker behaviour: ( 1) queens suppress reproduction by subordinates, which then forage, and ( 2) small-bodied females are handicapped as reproductives, and therefore take on a foraging role to assist a more fertile relative ( the 'subfertility' hypothesis). We removed queens from 19 nests and found that the remaining foragers enlarged their ovaries and reproduced at the same rate as solitary reproductives from unmanipulated (nonremoval) nests. This observation suggests that queen dominance limited reproduction by subordinates, and that foragers were not handicapped reproductives. To investigate the effect of body size variation on reproductive rate in the absence of social interactions, we placed single, newly eclosed females into 31 observation nests. Body size was not correlated with reproductive output or with the females' tenure in the observation nests. Nor was there any correlation between body size and number of brood cells in 21 solitary-female nonremoval nests. Taken together these data show that small females were not inherently poor reproductives. We also found that ovaries of reproductive females from social groups were larger than those of solitary reproductives, suggesting that social structure shapes ovary development. (C) 2009 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved.
C1 [Kapheim, Karen M.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
[O'Donnell, Sean] Univ Washington, Dept Psychol, Anim Behav Area, Seattle, WA 98195 USA.
RP Smith, AR (reprint author), Smithsonian Trop Res Inst, DPO AA, MRC 0580-12,Unit 9100,Box 0948, Miami, FL 34002 USA.
EM arsmith2@gmail.com
FU National Science Foundation (NSF) [NSF-IBN 0347315]; Smithsonian
Institution Postdoctoral Fellowship; Secretaria Nacional de Ciencia,
Tecnologia e Innovacion (SENACYT) of the Republic of Panama [COl06-003];
Smithsonian Tropical Research Institute (STRI); U.S. Department of
Education; UCLA EEB
FX A.R.S. was supported by the National Science Foundation (NSF)
International Research Fellowship Program, a Smithsonian Institution
Postdoctoral Fellowship and grant number COl06-003 ( to W. T. W. and A.
R. S.) from the Secretaria Nacional de Ciencia, Tecnologia e Innovacion
(SENACYT) of the Republic of Panama; research reported here was
developed from doctoral dissertation research submitted by A. R. S. to
the Animal Behavior Program at the University of Washington. S.O'D. was
supported by NSF grant NSF-IBN 0347315; K. M. K. was supported by a
Smithsonian Tropical Research Institute (STRI) Short-term Fellowship, a
U.S. Department of Education GAANN fellowship and a Holmes O. Miller
Fellowship from UCLA EEB; and W. T. W. was supported by STRI and the
Smithsonian Institution's Baird Restricted Endowment. Margarita
Lopez-Uribe, Julian Medina-Gutierrez, Dyana LaRosa and Ricardo Cossio
assisted in nest collection and observation nest censuses as interns
with support from STRI to W.T.W., and Michael Reiser did so with support
from a STRI Short-term Fellowship. Research on BCI was conducted under
scientific permit no. 75-99 from the Autoridad Nacional del Ambiente, in
accordance with the laws of the Republic of Panama. We thank two
anonymous referees for their comments that helped improved the
manuscript.
NR 50
TC 20
Z9 20
U1 2
U2 12
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
J9 ANIM BEHAV
JI Anim. Behav.
PD NOV
PY 2009
VL 78
IS 5
BP 1043
EP 1050
DI 10.1016/j.anbehav.2009.06.032
PG 8
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA 510OK
UT WOS:000271099200005
ER
PT J
AU Fleming, TH
Geiselman, C
Kress, WJ
AF Fleming, Theodore H.
Geiselman, Cullen
Kress, W. John
TI The evolution of bat pollination: a phylogenetic perspective
SO ANNALS OF BOTANY
LA English
DT Review
DE Angiosperms; nectar-feeding bats; plant phylogeny; pollen dispersal;
pollination modes
ID NECTAR-FEEDING BATS; ARCHAIC COEVOLUTIONARY SYSTEM; CEIBA-PENTANDRA
BOMBACACEAE; TROPICAL RAIN-FORESTS; FLOWER-VISITING BATS;
PAPUA-NEW-GUINEA; NEW-SOUTH-WALES; SYCONYCTERIS-AUSTRALIS; FLYING FOXES;
BLOSSOM BAT
AB Background Most tropical and subtropical plants are biotically pollinated, and insects are the major pollinators. A small but ecologically and economically important group of plants classified in 28 orders, 67 families and about 528 species of angiosperms are pollinated by nectar-feeding bats. From a phylogenetic perspective this is a derived pollination mode involving a relatively large and energetically expensive pollinator. Here its ecological and evolutionary consequences are explored.
Scope and Conclusions This review summarizes adaptations in bats and plants that facilitate this interaction and discusses the evolution of bat pollination from a plant phylogenetic perspective. Two families of bats contain specialized flower visitors, one in the Old World and one in the New World. Adaptation to pollination by bats has evolved independently many times from a variety of ancestral conditions, including insect-, bird- and non-volant mammal-pollination. Bat pollination predominates in very few families but is relatively common in certain angiosperm subfamilies and tribes. We propose that flower-visiting bats provide two important benefits to plants: they deposit large amounts of pollen and a variety of pollen genotypes on plant stigmas and, compared with many other pollinators, they are long-distance pollen dispersers. Bat pollination tends to occur in plants that occur in low densities and in lineages producing large flowers. In highly fragmented tropical habitats, nectar bats play an important role in maintaining the genetic continuity of plant populations and thus have considerable conservation value.
C1 [Fleming, Theodore H.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
[Geiselman, Cullen] New York Bot Garden, Inst Systemat Bot, Bronx, NY 10458 USA.
[Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
RP Fleming, TH (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
EM tedfleming@dakotacom.net
FU US National Science Foundation; National Geographic Society; Ted Turner
Foundation; Smithsonian Institution
FX We dedicate this review to the memory of Otto von Helversen for his
substantial contributions to our knowledge of bat pollination.
NR 193
TC 80
Z9 85
U1 19
U2 98
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0305-7364
J9 ANN BOT-LONDON
JI Ann. Bot.
PD NOV
PY 2009
VL 104
IS 6
BP 1017
EP 1043
DI 10.1093/aob/mcp197
PG 27
WC Plant Sciences
SC Plant Sciences
GA 510QX
UT WOS:000271106700001
PM 19789175
ER
PT J
AU Dawson, KS
Aldering, G
Amanullah, R
Barbary, K
Barrientos, LF
Brodwin, M
Connolly, N
Dey, A
Doi, M
Donahue, M
Eisenhardt, P
Ellingson, E
Faccioli, L
Fadeyev, V
Fakhouri, HK
Fruchter, AS
Gilbank, DG
Gladders, MD
Goldhaber, G
Gonzalez, AH
Goobar, A
Gude, A
Hattori, T
Hoekstra, H
Huang, X
Ihara, Y
Jannuzi, BT
Johnston, D
Kashikawa, K
Koester, B
Konishi, K
Kowalski, M
Lidman, C
Linder, EV
Lubin, L
Meyers, J
Morokuma, T
Munshi, F
Mullis, C
Oda, T
Panagia, N
Perlmutter, S
Postman, M
Pritchard, T
Rhodes, J
Rosati, P
Rubin, D
Schlegel, DJ
Spadafora, A
Stanford, SA
Stanishev, V
Stern, D
Strovink, M
Suzuki, N
Takanashi, N
Tokita, K
Wagner, M
Wang, L
Yasuda, N
Yee, HKC
AF Dawson, K. S.
Aldering, G.
Amanullah, R.
Barbary, K.
Barrientos, L. F.
Brodwin, M.
Connolly, N.
Dey, A.
Doi, M.
Donahue, M.
Eisenhardt, P.
Ellingson, E.
Faccioli, L.
Fadeyev, V.
Fakhouri, H. K.
Fruchter, A. S.
Gilbank, D. G.
Gladders, M. D.
Goldhaber, G.
Gonzalez, A. H.
Goobar, A.
Gude, A.
Hattori, T.
Hoekstra, H.
Huang, X.
Ihara, Y.
Jannuzi, B. T.
Johnston, D.
Kashikawa, K.
Koester, B.
Konishi, K.
Kowalski, M.
Lidman, C.
Linder, E. V.
Lubin, L.
Meyers, J.
Morokuma, T.
Munshi, F.
Mullis, C.
Oda, T.
Panagia, N.
Perlmutter, S.
Postman, M.
Pritchard, T.
Rhodes, J.
Rosati, P.
Rubin, D.
Schlegel, D. J.
Spadafora, A.
Stanford, S. A.
Stanishev, V.
Stern, D.
Strovink, M.
Suzuki, N.
Takanashi, N.
Tokita, K.
Wagner, M.
Wang, L.
Yasuda, N.
Yee, H. K. C.
CA Supernova Cosmology Project
TI AN INTENSIVE HUBBLE SPACE TELESCOPE* SURVEY FOR z > 1 TYPE Ia SUPERNOVAE
BY TARGETING GALAXY CLUSTERS
SO ASTRONOMICAL JOURNAL
LA English
DT Review
DE cosmology: observations; supernovae: general
ID COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT CLUSTERS; LIGHT-CURVE SHAPES;
IRAC SHALLOW SURVEY; SIMILAR-TO 1; X-RAY; RED-SEQUENCE; SPECTROSCOPIC
CONFIRMATION; LEGACY SURVEY; DARK ENERGY
AB We present a new survey strategy to discover and study high-redshift Type Ia supernovae (SNe Ia) using the Hubble Space Telescope (HST). By targeting massive galaxy clusters at 0.9 < z < 1.5, we obtain a twofold improvement in the efficiency of finding SNe compared to an HST field survey and a factor of 3 improvement in the total yield of SN detections in relatively dust-free red-sequence galaxies. In total, sixteen SNe were discovered at z > 0.95, nine of which were in galaxy clusters. This strategy provides an SN sample that can be used to decouple the effects of host-galaxy extinction and intrinsic color in high-redshift SNe, thereby reducing one of the largest systematic uncertainties in SN cosmology.
C1 [Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Dawson, K. S.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Linder, E. V.; Meyers, J.; Perlmutter, S.; Pritchard, T.; Rubin, D.; Schlegel, D. J.; Spadafora, A.; Strovink, M.; Suzuki, N.; Wagner, M.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Amanullah, R.; Barbary, K.; Fakhouri, H. K.; Goldhaber, G.; Gude, A.; Huang, X.; Meyers, J.; Munshi, F.; Perlmutter, S.; Pritchard, T.; Rubin, D.; Strovink, M.; Wagner, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Barrientos, L. F.] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA.
[Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Doi, M.; Ihara, Y.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Tokyo 1810015, Japan.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Eisenhardt, P.; Johnston, D.; Rhodes, J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ellingson, E.] Univ Colorado, Ctr Astrophys & Space Astron, UCB 389, Boulder, CO 80309 USA.
[Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA.
[Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Goobar, A.; Stanishev, V.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Hoekstra, H.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada.
[Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Johnston, D.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Kashikawa, K.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan.
[Kowalski, M.] Humboldt Univ, Inst Phys, Berlin, Germany.
[Lidman, C.] European So Observ, Santiago 19, Chile.
[Lubin, L.; Stanford, S. A.] Univ Calif Davis, Davis, CA 95618 USA.
[Mullis, C.] Wachovia Corp, Winston Salem, NC 27101 USA.
[Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Rhodes, J.] CALTECH, Pasadena, CA 91125 USA.
[Rosati, P.] ESO, D-85748 Garching, Germany.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Stanishev, V.] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal.
[Wang, L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Dawson, KS (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
EM kdawson@physics.utah.edu
RI Donahue, Megan/B-5361-2012; Yasuda, Naoki/A-4355-2011; Kowalski,
Marek/G-5546-2012; Stanishev, Vallery/M-8930-2013; Perlmutter,
Saul/I-3505-2015;
OI Stanishev, Vallery/0000-0002-7626-1181; Perlmutter,
Saul/0000-0002-4436-4661; Meyers, Joshua/0000-0002-2308-4230; Hoekstra,
Henk/0000-0002-0641-3231
NR 105
TC 45
Z9 46
U1 0
U2 5
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 NOV
PY 2009
VL 138
IS 5
BP 1271
EP 1283
DI 10.1088/0004-6256/138/5/1271
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 507KM
UT WOS:000270852100007
ER
PT J
AU Dupree, AK
Smith, GH
Strader, J
AF Dupree, A. K.
Smith, Graeme H.
Strader, Jay
TI FAST WINDS AND MASS LOSS FROM METAL-POOR FIELD GIANTS
SO ASTRONOMICAL JOURNAL
LA English
DT Review
DE stars: chromospheres; stars: Population II; stars: winds, outflows
ID HORIZONTAL-BRANCH STARS; GALACTIC GLOBULAR-CLUSTERS; COLOR-MAGNITUDE
DIAGRAM; DWARF COOLING SEQUENCE; X-RAY-EMISSION; RED-GIANT;
OMEGA-CENTAURI; INTRACLUSTER MEDIUM; CHROMOSPHERIC LINE; WHITE-DWARFS
AB Echelle spectra of the infrared He I lambda 10830 line were obtained with NIRSPEC on the Keck 2 telescope for 41 metal-deficient field giant stars including those on the red giant branch (RGB), asymptotic giant branch (AGB), and red horizontal branch (RHB). The presence of this He I line is ubiquitous in stars with T(eff) greater than or similar to 4500 K and MV fainter than -1.5, and reveals the dynamics of the atmosphere. The line strength increases with effective temperature for T(eff) greater than or similar to 5300 K in RHB stars. In AGB and RGB stars, the line strength increases with luminosity. Fast outflows (greater than or similar to 60 km s(-1)) are detected from the majority of the stars and about 40% of the outflows have sufficient speed as to allow escape of material from the star as well as from a globular cluster. Outflow speeds and line strengths do not depend on metallicity for our sample ([Fe/H]= -0.7 to -3.0), suggesting the driving mechanism for these winds derives from magnetic and/or hydrodynamic processes. Gas outflows are present in every luminous giant, but are not detected in all stars of lower luminosity indicating possible variability. Mass loss rates ranging from similar to 3 x 10(-10) to similar to 6 x 10(-8) M(circle dot) yr(-1) estimated from the Sobolev approximation for line formation represent values with evolutionary significance for red giants and RHB stars. We estimate that 0.2 M(circle dot) will be lost on the RGB, and the torque of this wind can account for observations of slowly rotating RHB stars in the field. About 0.1-0.2 M(circle dot) will be lost on the RHB itself. This first empirical determination of mass loss on the RHB may contribute to the appearance of extended horizontal branches in globular clusters. The spectra appear to resolve the problem of missing intracluster material in globular clusters. Opportunities exist for "wind smothering" of dwarf stars by winds from the evolved population, possibly leading to surface pollution in regions of high stellar density.
C1 [Dupree, A. K.; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Smith, Graeme H.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dupree@cfa.harvard.edu; graeme@ucolick.org; jstrader@cfa.harvard.edu
NR 124
TC 36
Z9 36
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2009
VL 138
IS 5
BP 1485
EP 1501
DI 10.1088/0004-6256/138/5/1485
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 507KM
UT WOS:000270852100023
ER
PT J
AU Jorgensen, JK
van Dishoeck, EF
Visser, R
Bourke, TL
Wilner, DJ
Lommen, D
Hogerheijde, MR
Myers, PC
AF Jorgensen, J. K.
van Dishoeck, E. F.
Visser, R.
Bourke, T. L.
Wilner, D. J.
Lommen, D.
Hogerheijde, M. R.
Myers, P. C.
TI PROSAC: a submillimeter array survey of low-mass protostars II. The mass
evolution of envelopes, disks, and stars from the Class 0 through I
stages
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; stars: circumstellar matter; stars: planetary systems:
protoplanetary disks; radiative transfer
ID YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DUST DISKS; MOLECULAR CLOUD CORES;
SPITZER C2D SURVEY; RHO-OPHIUCHI; CONTINUUM EMISSION; PROTOSTELLAR
ACCRETION; UNBIASED SUBMILLIMETER; INTERSTELLAR CLOUDS; SUBARCSECOND
SURVEY
AB Context. The key question about early protostellar evolution is how matter is accreted from the large-scale molecular cloud, through the circumstellar disk onto the central star.
Aims. We constrain the masses of the envelopes, disks, and central stars of a sample of low-mass protostars and compare the results to theoretical models for the evolution of young stellar objects through the early protostellar stages.
Methods. A sample of 20 Class 0 and I protostars has been observed in continuum at (sub)millimeter wavelengths at high angular resolution (typically 2 '') with the submillimeter array. Using detailed dust radiative transfer models of the interferometric data, as well as single-dish continuum observations, we have developed a framework for disentangling the continuum emission from the envelopes and disks, and from that estimated their masses. For the Class I sources in the sample HCO(+) 3-2 line emission was furthermore observed with the submillimeter array. Four of these sources show signs of Keplerian rotation, making it possible to determine the masses of the central stars. In the other sources the disks are masked by optically thick envelope and outflow emission.
Results. Both Class 0 and I protostars are surrounded by disks with typical masses of about 0.05 M(circle dot), although significant scatter is seen in the derived disk masses for objects within both evolutionary stages. No evidence is found for a correlation between the disk mass and evolutionary stage of the young stellar objects. This contrasts the envelope mass, which decreases sharply from similar to 1 M(circle dot) in the Class 0 stage to less than or similar to 0.1 M(circle dot) in the Class I stage. Typically, the disks have masses that are 1-10% of the corresponding envelope masses in the Class 0 stage and 20-60% in the Class I stage. For the Class I sources for which Keplerian rotation is seen, the central stars contain 70-98% of the total mass in the star-disk-envelope system, confirming that these objects are late in their evolution through the embedded protostellar stages, with most of the material from the ambient envelope accreted onto the central star. Theoretical models tend to overestimate the disk masses relative to the stellar masses in the late Class I stage.
Conclusions. The results argue in favor of a picture in which circumstellar disks are formed early during the protostellar evolution (although these disks are not necessarily rotationally supported) and rapidly process material accreted from the larger scale envelope onto the central star.
C1 [Jorgensen, J. K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[van Dishoeck, E. F.; Visser, R.; Lommen, D.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bourke, T. L.; Wilner, D. J.; Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Jorgensen, JK (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
EM jes@astro.uni-bonn.de
RI Visser, Ruud/J-8574-2012
FU Canadian Space Agency; Netherlands Organization for Scientific Research
(NWO); NOVA; NASA [NNX09AB89G]
FX We thank the referee for good suggestions about the presentation of
these results. It is also a pleasure to thank the Submillimeter Array
sta. for help in carrying out observations and technical assistance with
the resulting data. The Submillimeter Array is a joint project between
the Smithsonian Astrophysical Observatory and the Academia Sinica
Institute of Astronomy and Astrophysics, and is funded by the
Smithsonian Institution and the Academia Sinica. This research was based
in part on observations from the James Maxwell Telescope archive at the
Canadian Astronomy Data Centre operated by the National Research Council
of Canada with the support of the Canadian Space Agency. It is also used
observations made with the NASA/ESA Hubble Space Telescope, obtained
from the data archive at the Space Telescope Institute. STScI is
operated by the association of Universities for Research in Astronomy,
Inc. under the NASA contract NAS 5-26555. Astrochemistry in Leiden is
supported by a Spinoza Grant from the Netherlands Organization for
Scientific Research (NWO) and a NOVA grant. The research of T. L. B. was
supported by NASA Origins grant NNX09AB89G.
NR 93
TC 126
Z9 126
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2009
VL 507
IS 2
BP 861
EP U334
DI 10.1051/0004-6361/200912325
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 522VU
UT WOS:000272029000031
ER
PT J
AU Argiroffi, C
Maggio, A
Peres, G
Drake, JJ
Lopez-Santiago, J
Sciortino, S
Stelzer, B
AF Argiroffi, C.
Maggio, A.
Peres, G.
Drake, J. J.
Lopez-Santiago, J.
Sciortino, S.
Stelzer, B.
TI X-ray optical depth diagnostics of T Tauri accretion shocks
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: atmospheres; stars: coronae; stars: pre-main sequence;
techniques: spectroscopic; X-rays: stars
ID EMISSION MEASURE DISTRIBUTIONS; ACTIVE STELLAR CORONAE; XMM-NEWTON; DISK
ACCRETION; QUIESCENT STATES; BROWN DWARFS; SOLAR CORONA; YOUNG STARS;
SPECTROSCOPY; HYDRAE
AB Context. In classical T Tauri stars, X-rays are produced by two plasma components: a hot low-density plasma, with frequent flaring activity, and a high-density lower temperature plasma. The former is coronal plasma related to the stellar magnetic activity. The latter component, never observed in non-accreting stars, could be plasma heated by the shock formed by the accretion process. However its nature is still being debated.
Aims. Our aim is to probe the soft X-ray emission from the high-density plasma component in classical T Tauri stars to check whether this plasma is heated in the accretion shock or whether it is coronal plasma.
Methods. High-resolution X-ray spectroscopy allows us to measure individual line fluxes. We analyze X-ray spectra of the classical T Tauri stars MP Muscae and TW Hydrae. Our aim is to evaluate line ratios to search for optical depth effects, which are expected in the accretion-driven scenario. We also derive the plasma emission measure distributions EMD, to investigate whether and how the EMD of accreting and non accreting young stars differ. The results are compared to those obtained for the non-accreting weak-line T Tauri star TWA 5.
Results. We find evidence of resonance scattering in the strongest lines of MP Mus, supporting the idea that soft X-rays are produced by plasma heated in the accretion shock. We also find that the EMD of MP Mus has two peaks: a cool peak at temperatures expected for plasma heated in the accretion shock, and a hot peak typical of coronal plasma. The shape of the EMD of MP Mus appears to be the superposition of the EMD of a pure coronal source, like TWA 5, and an EMD alike that of TW Hya, which is instead dominated by shock-heated plasma.
C1 [Argiroffi, C.; Peres, G.] Univ Palermo, Sez Astron, Dipartimento Sci Fisiche & Astron, I-90134 Palermo, Italy.
[Argiroffi, C.; Maggio, A.; Peres, G.; Sciortino, S.; Stelzer, B.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy.
[Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lopez-Santiago, J.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis & Ciencias Atmosfera, E-28040 Madrid, Spain.
RP Argiroffi, C (reprint author), Univ Palermo, Sez Astron, Dipartimento Sci Fisiche & Astron, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM argi@astropa.unipa.it; maggio@astropa.inaf.it; peres@astropa.unipa.it;
jdrake@cfa.harvard.edu; jls@astrax.fis.ucm.es; sciorti@astropa.inaf.it;
stelzer@astropa.inaf.it
RI Maggio, Antonio/P-5700-2015;
OI Maggio, Antonio/0000-0001-5154-6108; PERES,
Giovanni/0000-0002-6033-8180; ARGIROFFI, Costanza/0000-0003-2073-1348
FU ASI-INAF [I/023/05/0]; Ministero dell'Universita e della Ricerca; NASA
[NAS8-39073]; Comunidad Autonoma de Madrid [S-0505/ESP-0237]; Spanish
Ministerio de Ciencia y Tecnologia [AYA2008-06423-C03-03]; ESA Member
States
FX The authors thank the referee, M. Gudel, for comments that improved the
paper. The authors are grateful to G. G. Sacco for providing the results
of the accretion shock simulations. C. A., A. M., G. P., S. S., and B.
S. acknowledge partial support for this work from contract ASI-INAF
I/023/05/0 and from the Ministero dell'Universita e della Ricerca. J. J.
D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center
during the course of this research, and thanks the director, H.
Tananbaum, and CXC science team for advice and support. J. L. S.
acknowledges financial support by the projects S-0505/ESP-0237
(ASTROCAM) of the Comunidad Autonoma de Madrid and AYA2008-06423-C03-03
of the Spanish Ministerio de Ciencia y Tecnologia. Based on observations
obtained with XMM-Newton, an ESA science mission with instruments and
contributions directly funded by ESA Member States and NASA.
NR 63
TC 15
Z9 15
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 NOV
PY 2009
VL 507
IS 2
BP 939
EP 948
DI 10.1051/0004-6361/200912792
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 522VU
UT WOS:000272029000038
ER
PT J
AU in 't Zand, JJM
Jonker, PG
Bassa, CG
Markwardt, CB
Levine, AM
AF in 't Zand, J. J. M.
Jonker, P. G.
Bassa, C. G.
Markwardt, C. B.
Levine, A. M.
TI Monitoring campaign of 1RXS J171824.2-402934, the low-mass X-ray binary
with the lowest mass accretion rate
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; stars: neutron; X-rays: binaries; X-rays:
individuals: 1RXS J171824.2-402934; X-rays: individuals: RX J1718.4-4029
ID PHOTOMETRIC STANDARD STARS; RESOLUTION CAMERA HRC; ALL-SKY SURVEY;
GALACTIC-CENTER; ULTRACOMPACT BINARIES; TIMING-EXPLORER; DISCOVERY;
TRANSIENTS; CATALOG; CALIBRATION
AB An X-ray monitoring campaign with Chandra and Swift confirms that 1RXS J171824.2-402934 is accreting at the lowest rate among the known persistently accreting low-mass X-ray binaries. A thermonuclear X-ray burst was detected with the all-sky monitor on RXTE. This is only the second such burst seen in 1RXS J171824.2-402934 in more than 20 Ms of observations done over 19 years. The low burst recurrence rate is in line with the low accretion rate. The persistent nature and low accretion rate can be reconciled within accretion disk theory if the binary system is ultracompact. An unprecedentedly short orbital period of less than approximate to 7 min would be implied. An ultracompact nature, together with the properties of the type I X-ray burst, suggests, in turn, that helium-rich material is accreted. Optical follow-up of the Chandra error region does not reveal an unambiguous counterpart.
C1 [in 't Zand, J. J. M.; Jonker, P. G.; Bassa, C. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bassa, C. G.] Radboud Univ Nijmegen, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Levine, A. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP in 't Zand, JJM (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM jeanz@sron.nl
NR 50
TC 8
Z9 8
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 NOV
PY 2009
VL 506
IS 2
BP 857
EP 863
DI 10.1051/0004-6361/200912403
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514DP
UT WOS:000271374800034
ER
PT J
AU van Weeren, RJ
Rottgering, HJA
Bagchi, J
Raychaudhury, S
Intema, HT
Miniati, F
Ensslin, TA
Markevitch, M
Erben, T
AF van Weeren, R. J.
Roettgering, H. J. A.
Bagchi, J.
Raychaudhury, S.
Intema, H. T.
Miniati, F.
Ensslin, T. A.
Markevitch, M.
Erben, T.
TI Radio observations of ZwCl 2341.1+0000: a double radio relic cluster
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radio continuum: galaxies; galaxies: active; galaxies: clusters:
individual: ZwCl 2341.1+0000; cosmology: large-scale structure of
Universe
ID LARGE-SCALE STRUCTURE; X-RAY-EMISSION; SHOCK ACCELERATION; COSMIC-RAYS;
GALAXY CLUSTERS; MAGNETIC-FIELDS; TELESCOPE OBSERVATIONS;
PARTICLE-ACCELERATION; ASTROPHYSICAL SHOCKS; COMA CLUSTER
AB Context. Hierarchal models of large-scale structure (LSS) formation predict that galaxy clusters grow via gravitational infall and mergers of smaller subclusters and galaxy groups. Diffuse radio emission, in the form of radio halos and relics, is found in clusters undergoing a merger, indicating that shocks or turbulence associated with the merger are capable of accelerating electrons to highly relativistic energies. Double relics are a rare class of radio sources found in the periphery of clusters, with the two components located symmetrically on the opposite sides of the cluster center. These relics are important probes of the cluster periphery as (i) they provide an estimate of the magnetic field strength, and (ii) together with detailed modeling can be used to derive information about the merger geometry, mass, and timescale. Observations of these double relics can thus be used to test the framework of LSS formation. Here we report on radio observations of ZwCl 2341.1+0000, a complex merging structure of galaxies located at z = 0.27, using Giant Metrewave Radio Telescope (GMRT) observations.
Aims. The main aim of the observations is to study the nature of the diffuse radio emission in the galaxy cluster ZwCl 2341.1+0000.
Methods. We carried out GMRT 610, 241, and 157 MHz continuum observations of ZwCl 2341.1+0000. The radio observations are combined with X-ray and optical data of the cluster.
Results. The GMRT observations show a double peripheral radio relic in the cluster ZwCl 2341.1+0000. The spectral index is -0.49 +/- 0.18 for the northern relic and -0.76 +/- 0.17 for the southern relic. We have derived values of 0.48-0.93 mu Gauss for the equipartition magnetic field strength. The relics are probably associated with outward traveling merger shock waves.
C1 [van Weeren, R. J.; Roettgering, H. J. A.; Intema, H. T.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bagchi, J.] IUCAA, Pune 411007, Maharashtra, India.
[Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Miniati, F.] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Ensslin, T. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Erben, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
RP van Weeren, RJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM rvweeren@strw.leidenuniv.nl
RI Intema, Huib/D-1438-2012;
OI Intema, Huib/0000-0002-5880-2730; van Weeren,
Reinout/0000-0002-0587-1660
FU Royal Netherlands Academy of Arts and Sciences; Alfred P. Sloan
Foundation; Participating Institutions; National Science Foundation; U.
S. Department of Energy; National Aeronautics and Space Administration;
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England
FX 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 VizieR
catalogue access tool, CDS, Strasbourg, France.
NR 75
TC 41
Z9 41
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2009
VL 506
IS 3
BP 1083
EP U46
DI 10.1051/0004-6361/200912287
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 516AV
UT WOS:000271514900006
ER
PT J
AU Read, AM
Saxton, RD
Jonker, PG
Kuulkers, E
Esquej, P
Pojmanski, G
Torres, MAP
Goad, MR
Freyberg, MJ
Modjaz, M
AF Read, A. M.
Saxton, R. D.
Jonker, P. G.
Kuulkers, E.
Esquej, P.
Pojmanski, G.
Torres, M. A. P.
Goad, M. R.
Freyberg, M. J.
Modjaz, M.
TI XMMSL1 J060636.2-694933: an XMM-Newton slew discovery and Swift/Magellan
follow up of a new classical nova in the LMC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: novae, cataclysmic variables; stars: individual: XMMSL1
J060636.2-694933; surveys; X-rays: general
ID LARGE-MAGELLANIC-CLOUD; X-RAY-EMISSION; V1974 CYGNI; SPECTRA; CATALOG;
STARS; EVOLUTION; OUTBURST; DISTANCE; MODELS
AB Aims. In order to discover new X-ray transients, the data taken by XMM-Newton as it slews between targets are being processed and cross-correlated with other X-ray observations.
Methods. A bright source, XMMSL1 J060636.2-694933, was detected on 18 July 2006 at a position where no previous X-ray source had been seen. The XMM-Newton slew data, plus follow-up dedicated XMM-Newton and Swift observations, plus optical data acquired with the Magellan Clay telescope, and archival All-Sky Automated Survey (ASAS) data were used to classify the new object, and to investigate its properties.
Results. No XMM-Newton slew X-ray counts are detected above 1 keV and the source is seen to be over five hundred times brighter than the ROSAT All-Sky Survey upper limit at that position. The line-rich optical spectrum acquired with the Magellan telescope allows the object to be classified as an A(0) auroral phase nova, and the soft X-ray spectrum indicates that the nova was in a super-soft source state in the X-ray decline seen in the follow-up X-ray observations. The archival ASAS data suggests that the nova at onset (Oct 2005) was a "very fast" nova, and an estimate of its distance is consistent with the nova being situated within the LMC.
Conclusions. With the discovery presented here of a new classical nova in the LMC, it is clear that XMM-Newton slew data are continuing to offer a powerful opportunity to find new X-ray transient objects.
C1 [Read, A. M.; Esquej, P.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Saxton, R. D.; Kuulkers, E.] ESAC, XMM Newton SOC, Madrid 28691, Spain.
[Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pojmanski, G.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Freyberg, M. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Modjaz, M.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
RP Read, AM (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM amr30@star.le.ac.uk
FU ESA Member States; USA (NASA); Bundesministerium fur Wirtschaft und
Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50
OX 0001]; Max-Planck Society; Heidenhain-Stiftung; STFC; PGJ of the
Netherlands Organisation for Scientific Research; MNiSzW
[N2030731/1328]; Miller Institute Research Fellowship
FX The XMM-Newton project is an ESA Science Mission with instruments and
contributions directly funded by ESA Member States and the USA (NASA).
The XMM-Newton project is supported by the Bundesministerium fur
Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt
(BMWI/DLR, FKZ 50 OX 0001), the Max-Planck Society and the
Heidenhain-Stiftung. AMR and PE acknowledge the support of STFC funding,
and PGJ of the Netherlands Organisation for Scientific Research. The
ASAS project is supported by the N2030731/1328 grant from the MNiSzW. We
thank the referee (G. Sala) for very useful comments and several
references that have improved the paper notably. We thank Kim Page for
providing the white dwarf atmosphere model, and we thank her and Graham
Wynn for useful discussions. The use of the spectral analysis software
package MOLLY written by Tom Marsh is also acknowledged. M. M.
acknowledges support by a Miller Institute Research Fellowship during
the time in which part of the work was completed.
NR 36
TC 5
Z9 5
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD NOV
PY 2009
VL 506
IS 3
BP 1309
EP 1317
DI 10.1051/0004-6361/200912082
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 516AV
UT WOS:000271514900023
ER
PT J
AU Toft, S
Franx, M
van Dokkum, P
Schreiber, NMF
Labbe, I
Wuyts, S
Marchesini, D
AF Toft, S.
Franx, M.
van Dokkum, P.
Schreiber, N. M. Foerster
Labbe, I.
Wuyts, S.
Marchesini, D.
TI THE SIZE-STAR FORMATION RELATION OF MASSIVE GALAXIES AT 1.5 < z < 2.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: high-redshift
ID ULTRA DEEP FIELD; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES;
DIGITAL SKY SURVEY; ELLIPTIC GALAXIES; SUBMILLIMETER GALAXIES;
EXTRAGALACTIC SURVEY; QUIESCENT GALAXIES; EVOLUTION; COMPACT
AB We study the relation between size and star formation activity in a complete sample of 225 massive (M* > 5 x 10(10) M(circle dot)) galaxies at 1.5 < z < 2.5, selected from the FIREWORKS UV-IR catalog of the CDFS. Based on stellar population synthesis model fits to the observed rest-frame UV-NIR spectral energy distributions, and independent MIPS 24 mu m observations, 65% of the galaxies are actively forming stars, while 35% are quiescent. Using sizes derived from two-dimensional surface brightness profile fits to high-resolution (FWHM(PSF) similar to 0".45) ground-based ISAAC data, we confirm and improve the significance of the relation between star formation activity and compactness found in previous studies, using a large, complete mass-limited sample. At z similar to 2, massive quiescent galaxies are significantly smaller than massive star-forming galaxies, and a median factor of 0.34 similar to +/- 0.02 smaller than galaxies of similar mass in the local universe. Thirteen percent of the quiescent galaxies are unresolved in the ISAAC data, corresponding to sizes <1 kpc, more than five times smaller than galaxies of similar mass locally. The quiescent galaxies span a Kormendy relation which, compared to the relation for local early types, is shifted to smaller sizes and brighter surface brightnesses and is incompatible with passive evolution. The progenitors of the quiescent galaxies were likely dominated by highly concentrated, intense nuclear starbursts at z similar to 3-4, in contrast to star-forming galaxies at z similar to 2 which are extended and dominated by distributed star formation.
C1 [Toft, S.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Toft, S.] European So Observ, D-85748 Garching, Germany.
[Franx, M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dokkum, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Schreiber, N. M. Foerster] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Labbe, I.] Carnegie Observ, Pasadena, CA 91101 USA.
[Wuyts, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marchesini, D.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
RP Toft, S (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Mariesvej 30, DK-2100 Copenhagen, Denmark.
EM sune@dark-cosmology.dk; franx@strw.leidenuniv.nl; dokkum@astro.yale.edu;
forster@mpe.mpg.de; ivo@ociw.edu; swuyts@cfa.harvard.edu;
danilo.marchesini@tufts.edu
FU Lundbeck Foundation; W. M. Keck Foundation
FX We thank Thomas R. Greve, Steffen Mieske, and Mariska Kriek for useful
discussions, and the anonymous referee, for useful suggestions which
improved the analysis. S. Toft gratefully acknowledges support from the
Lundbeck Foundation. S. Wuyts gratefully acknowledges support from the
W. M. Keck Foundation.
NR 49
TC 42
Z9 42
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2009
VL 705
IS 1
BP 255
EP 260
DI 10.1088/0004-637X/705/1/255
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508CA
UT WOS:000270903200021
ER
PT J
AU Penev, K
Barranco, J
Sasselov, D
AF Penev, Kaloyan
Barranco, Joseph
Sasselov, Dimitar
TI DIRECT CALCULATION OF THE TURBULENT DISSIPATION EFFICIENCY IN ANELASTIC
CONVECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; convection; hydrodynamics; methods: numerical; stellar
dynamics; turbulence
ID SOLAR P-MODES; TIDAL CIRCULARIZATION; VISCOSITY; STARS; SIMULATIONS
AB The current understanding of the turbulent dissipation in stellar convective zones is based on the assumption that the turbulence follows Kolmogorov scaling. This assumption is valid for some cases in which the time frequency of the external shear is high (e.g., solar p modes). However, for many cases of astrophysical interest (e.g., binary orbits, stellar pulsations, etc.), the timescales of interest lie outside the regime of applicability of Kolmogorov scaling. We present direct calculations of the dissipation efficiency of the turbulent convective flow in this regime, using simulations of anelastic convection with external forcing. We show that the effects of the turbulent flow are well represented by an effective viscosity coefficient, we provide the values of the effective viscosity as a function of the perturbation frequency and compare our results to the perturbative method for finding the effective viscosity of Penev et al. that can be applied to actual simulations of the surface convective zones of stars.
C1 [Penev, Kaloyan] Harvard Univ, Cambridge, MA 02138 USA.
[Barranco, Joseph] San Francisco State Univ, San Francisco, CA 94132 USA.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Penev, K (reprint author), Harvard Univ, 60 Garden St,Mail Stop 10, Cambridge, MA 02138 USA.
OI Barranco, Joseph/0000-0003-2045-677X
NR 17
TC 16
Z9 16
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2009
VL 705
IS 1
BP 285
EP 297
DI 10.1088/0004-637X/705/1/285
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508CA
UT WOS:000270903200024
ER
PT J
AU Cohen, O
Attrill, GDR
Manchester, WB
Wills-Davey, MJ
AF Cohen, Ofer
Attrill, Gemma D. R.
Manchester, Ward B.
Wills-Davey, Meredith J.
TI NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY
13 CME EVENT OBSERVED BY STEREO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE MHD; Sun: corona; Sun: coronal mass ejections (CMEs)
ID ULTRAVIOLET IMAGING TELESCOPE; 1997 MAGNETIC CLOUD; SOLAR-FLARE WAVES;
EIT WAVES; MASS EJECTION; SOHO/EIT OBSERVATIONS; LASCO OBSERVATIONS;
MORETON/EIT WAVE; DIMMING REGIONS; MHD WAVES
AB On 2009 February 13, a coronal wave-CME-dimming event was observed in quadrature by the Solar Terrestrial Relations Observatory (STEREO) spacecraft. We analyze this event using a three-dimensional, global magnetohydrodynamic model for the solar corona. The numerical simulation is driven and constrained by the observations, and indicates where magnetic reconnection occurs between the expanding CME core and surrounding environment. We focus primarily on the lower corona, extending out to 3 R(circle dot); this range allows simultaneous comparison with both EUVI and COR1 data. Our simulation produces a diffuse coronal bright front remarkably similar to that observed by STEREO/EUVI at 195 angstrom. It is made up of two components, and is the result of a combination of both wave and non-wave mechanisms. The CME becomes large-scale quite low (< 200 Mm) in the corona. It is not, however, an inherently large-scale event; rather, the expansion is facilitated by magnetic reconnection between the expanding CME core and the surrounding magnetic environment. In support of this, we also find numerous secondary dimmings, many far from the initial CME source region. Relating such dimmings to reconnecting field lines within the simulation provides further evidence that CME expansion leads to the "opening" of coronal field lines on a global scale. Throughout the CME expansion, the coronal wave maps directly to the CME footprint. Our results suggest that the ongoing debate over the "true" nature of diffuse coronal waves may be mischaracterized. It appears that both wave and non-wave models are required to explain the observations and understand the complex nature of these events.
C1 [Cohen, Ofer; Attrill, Gemma D. R.; Wills-Davey, Meredith J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Manchester, Ward B.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Manchester, Ward/I-9422-2012;
OI Cohen, Ofer/0000-0003-3721-0215
FU NSF [ATM-0823592]; NASA [NNX09AB11G-R]; [SP02H1701R]
FX We would like to thank an unknown referee for his/her comments and
suggestions. We thank Yang Liu and Hao Thai for providing the
magnetogram data, and Michelle Murray for suggestions about displaying
the simulation data. We also thank Pascal Demoulin, Nariaki Nitta-san,
Tibor Torok, and Veronica Ontiveros for helpful discussions. This work
has been supported by SHINE through NSF grant ATM-0823592 and the NASA
grant NNX09AB11G-R. We acknowledge the contract SP02H1701R from Lockheed
Martin to SAO. Simulation results were obtained using the Space Weather
Modeling Framework, developed by the Center for Space Environment
Modeling, at the University of Michigan with funding support from NASA
ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. SOHO is a project of
international cooperation between ESA & NASA. The STEREO/SECCHI data are
produced by an international consortium: NRL, LMSAL, NASA, GSFC (USA);
RAL ( UK); MPS CSL (Belgium); and IOTA, IAS (France).
NR 80
TC 96
Z9 97
U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2009
VL 705
IS 1
BP 587
EP 602
DI 10.1088/0004-637X/705/1/587
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508CA
UT WOS:000270903200048
ER
PT J
AU David, LP
Jones, C
Forman, W
Nulsen, P
Vrtilek, J
O'Sullivan, E
Giacintucci, S
Raychaudhury, S
AF David, Laurence P.
Jones, Christine
Forman, William
Nulsen, Paul
Vrtilek, Jan
O'Sullivan, Ewan
Giacintucci, Simona
Raychaudhury, Somak
TI ISOTROPIC ACTIVE GALACTIC NUCLEUS HEATING WITH SMALL RADIO-QUIET BUBBLES
IN THE NGC 5044 GROUP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cooling flows; intergalactic medium; galaxies: active; galaxies:
clusters: general; X-rays: galaxies: clusters
ID EARLY-TYPE GALAXIES; X-RAY SPECTROSCOPY; MULTIPHASE HOT GAS; ELLIPTIC
GALAXIES; COOLING-FLOW; CHANDRA OBSERVATIONS; HIGH-RESOLUTION;
XMM-NEWTON; BUOYANT BUBBLES; NGC-5044 GROUP
AB A Chandra observation of the X-ray bright group NGC 5044 shows that the X-ray emitting gas has been strongly perturbed by recent outbursts from the central active galactic nucleus (AGN) and also by motion of the central dominant galaxy relative to the group gas. The NGC 5044 group hosts many small radio-quiet cavities with a nearly isotropic distribution, cool filaments, a semi-circular cold front, and a two-armed spiral shaped feature of cool gas. A Giant Metrewave Radio Telescope (GMRT) observation of NGC 5044 at 610 MHz shows the presence of extended radio emission with a "torus-shaped" morphology. The largest X-ray filament appears to thread the radio torus, suggesting that the lower entropy gas within the filament is material being uplifted from the center of the group. The radio emission at 235 MHz is much more extended than the emission at 610 MHz, with little overlap between the two frequencies. One component of the 235 MHz emission passes through the largest X-ray cavity and is then deflected just behind the cold front. A second detached radio lobe is also detected at 235 MHz beyond the cold front. All of the smaller X-ray cavities in the center of NGC 5044 are undetected in the GMRT observations. Since the smaller bubbles are probably no longer momentum driven by the central AGN, their motion will be affected by the group "weather" as they buoyantly rise outward. Hence, most of the enthalpy within the smaller bubbles will likely be deposited near the group center and isotropized by the group weather. The total mechanical power of the smaller radio quiet cavities is P(c) = 9.2 x 10(41) erg s(-1) which is sufficient to suppress about one-half of the total radiative cooling within the central 10 kpc. This is consistent with the presence of Ha emission within this region which shows that at least some of the gas is able to cool. The mechanical heating power of the larger southern cavity, located between 10 and 20 kpc, is six times greater than the combined mechanical power of the smaller radio-quiet cavities and could suppress all radiative cooling within the central 25 kpc if the energy were deposited and isotropized within this region. Within the central 20 kpc, emission from low-mass X-ray binaries (LMXBs) is a significant component of the X-ray emission above 2 keV. The presence of hard X-ray emission from unresolved LMXBs makes it difficult to place strong constraints on the amount of shock heated gas within the X-ray cavities.
C1 [David, Laurence P.; Jones, Christine; Forman, William; Nulsen, Paul; Vrtilek, Jan; O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Giacintucci, Simona] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
RP David, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM david@head.cfa.harvard.edu
OI O'Sullivan, Ewan/0000-0002-5671-6900; Nulsen, Paul/0000-0003-0297-4493;
Forman, William/0000-0002-9478-1682
FU NASA [GO7-8127X]
FX We thank T. Venturi and R. Athreya for help with the GMRT observations
and M. Markevitch with information about the ACIS background. This work
was supported in part by NASA grant GO7-8127X.
NR 55
TC 56
Z9 56
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2009
VL 705
IS 1
BP 624
EP 638
DI 10.1088/0004-637X/705/1/624
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508CA
UT WOS:000270903200051
ER
PT J
AU Boyer, ML
McDonald, I
van Loon, JT
Gordon, KD
Babler, B
Block, M
Bracker, S
Engelbracht, C
Hora, J
Indebetouw, R
Meade, M
Meixner, M
Misselt, K
Oliveira, JM
Sewilo, M
Shiao, B
Whitney, B
AF Boyer, Martha L.
McDonald, Iain
van Loon, Jacco Th.
Gordon, Karl D.
Babler, Brian
Block, Miwa
Bracker, Steve
Engelbracht, Charles
Hora, Joe
Indebetouw, Remy
Meade, Marilyn
Meixner, Margaret
Misselt, Karl
Oliveira, Joana M.
Sewilo, Marta
Shiao, Bernie
Whitney, Barbara
TI DUST PRODUCTION AND MASS LOSS IN THE GALACTIC GLOBULAR CLUSTER NGC 362
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; globular clusters: individual (NGC 362); infrared:
stars; stars: AGB and post-AGB; stars: mass loss; stars: winds, outflows
ID SMALL-MAGELLANIC-CLOUD; INTRACLUSTER MEDIUM; OMEGA-CENTAURI; 2ND
PARAMETER; GIANT-BRANCH; RED GIANTS; AGB STARS; MODEL ATMOSPHERES;
IONIZED HYDROGEN; PROPER MOTIONS
AB We investigate dust production and stellar mass loss in the Galactic globular cluster NGC 362. Due to its close proximity to the Small Magellanic Cloud (SMC), NGC 362 was imaged with the Infrared Array Camera and Multiband Imaging Photometer cameras onboard the Spitzer Space Telescope as part of the Surveying the Agents of Galaxy Evolution (SAGE-SMC) Spitzer Legacy program. We detect several cluster members near the tip of the red giant branch (RGB) that exhibit infrared excesses indicative of circumstellar dust and find that dust is not present in measurable quantities in stars below the tip of the RGB. We modeled the spectral energy distribution ( SED) of the stars with the strongest IR excess and find a total cluster dustmass-loss rate of 3.0(-1.2)(+2.0) x 10(-9) M-circle dot yr(-1), corresponding to a gas mass-loss rate of 8.6(-3.4)(+5.6) x 10(-6)M(circle dot) yr(-1), assuming [Fe/H] = -1.16. This mass loss is in addition to any dustless mass loss that is certainly occurring within the cluster. The two most extreme stars, variables V2 and V16, contribute up to 45% of the total cluster dust-traced mass loss. The SEDs of the more moderate stars indicate the presence of silicate dust, as expected for low-mass, low-metallicity stars. Surprisingly, the SED shapes of the stars with the strongest mass-loss rates appear to require the presence of amorphous carbon dust, possibly in combination with silicate dust, despite their oxygen-rich nature. These results corroborate our previous findings in omega Centauri.
C1 [Boyer, Martha L.; Gordon, Karl D.; Meixner, Margaret; Sewilo, Marta; Shiao, Bernie; Whitney, Barbara] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[McDonald, Iain; van Loon, Jacco Th.; Oliveira, Joana M.] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Babler, Brian; Bracker, Steve; Meade, Marilyn] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Block, Miwa; Engelbracht, Charles; Misselt, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hora, Joe] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
RP Boyer, ML (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM mboyer@stsci.edu
OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650
FU Spitzer [1309827, 1340964]
FX We thank Jay Anderson for sharing the Hubble ACS image and Yoshifusa Ita
for sharing AKARI photometry and the mid-IR spectrum of star s02. We
also thank the referee for his or her helpful comments. This work was
supported by Spitzer via JPL contracts 1309827 and 1340964.
NR 62
TC 33
Z9 33
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 NOV 1
PY 2009
VL 705
IS 1
BP 746
EP 757
DI 10.1088/0004-637X/705/1/746
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508CA
UT WOS:000270903200062
ER
PT J
AU Risaliti, G
Braito, V
Laparola, V
Bianchi, S
Elvis, M
Fabbiano, G
Maiolino, R
Matt, G
Reeves, J
Salvati, M
Wang, J
AF Risaliti, G.
Braito, V.
Laparola, V.
Bianchi, S.
Elvis, M.
Fabbiano, G.
Maiolino, R.
Matt, G.
Reeves, J.
Salvati, M.
Wang, J.
TI A STRONG EXCESS IN THE 20-100 keV EMISSION OF NGC 1365
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC, 1365); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEUS; HARD X-RAYS; CHANDRA; TRANSMISSION; DISCOVERY;
GALAXY; AGN
AB We present a new Suzaku observation of the obscured active galactic nucleus in NGC 1365, revealing an unexpected excess of X-rays above 20 keV of at least a factor similar to 2 with respect to the extrapolation of the best-fitting 3-10 keV model. Additional Swift-BAT and Integral-IBIS observations show that the 20-100 keV is concentrated within similar to 1.5 arcmin from the center of the galaxy, and is not significantly variable on timescales from days to years. A comparison of this component with the 3-10 keV emission, which is characterized by a rapidly variable absorption, suggests a complex structure of the circumnuclear medium, consisting of at least two distinct components with rather different physical properties, one of which covers >80% of the source with a column density N-H similar to 3-4x10(24) cm(-2). An alternative explanation is the presence of a double active nucleus in the center of NGC 1365.
C1 [Risaliti, G.; Elvis, M.; Fabbiano, G.; Wang, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Risaliti, G.; Salvati, M.] INAF Osservatorio Arcetri, I-50125 Florence, Italy.
[Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Laparola, V.] INAF IASF, I-90146 Palermo, Italy.
[Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
[Maiolino, R.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Reeves, J.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM grisaliti@cfa.harvard.edu
RI Wang, Junfeng/A-1476-2011; Bianchi, Stefano/B-4804-2010; XRAY,
SUZAKU/A-1808-2009;
OI Bianchi, Stefano/0000-0002-4622-4240; Risaliti,
Guido/0000-0002-3556-977X; La Parola, Valentina/0000-0002-8087-6488;
Braito, Valentina/0000-0002-2629-4989
FU ASI-INAF [I/088/06/0]; NASA [NNX08AN48G]; [2006025203]
FX This work has been partly supported by grants prinmiur 2006025203,
ASI-INAF I/088/06/0, and NASA NNX08AN48G.
NR 21
TC 24
Z9 24
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 NOV 1
PY 2009
VL 705
IS 1
BP L1
EP L5
DI 10.1088/0004-637X/705/1/L1
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508JV
UT WOS:000270927900001
ER
PT J
AU Kessler, R
Becker, AC
Cinabro, D
Vanderplas, J
Frieman, JA
Marriner, J
Davis, TM
Dilday, B
Holtzman, J
Jha, SW
Lampeitl, H
Sako, M
Smith, M
Zheng, C
Nichol, RC
Bassett, B
Bender, R
Depoy, DL
Doi, M
Elson, E
Filippenko, AV
Foley, RJ
Garnavich, PM
Hopp, U
Ihara, Y
Ketzeback, W
Kollatschny, W
Konishi, K
Marshall, JL
McMillan, RJ
Miknaitis, G
Morokuma, T
Mortsell, E
Pan, K
Prieto, JL
Richmond, MW
Riess, AG
Romani, R
Schneider, DP
Sollerman, J
Takanashi, N
Tokita, K
van der Heyden, K
Wheeler, JC
Yasuda, N
York, D
AF Kessler, Richard
Becker, Andrew C.
Cinabro, David
Vanderplas, Jake
Frieman, Joshua A.
Marriner, John
Davis, Tamara M.
Dilday, Benjamin
Holtzman, Jon
Jha, Saurabh W.
Lampeitl, Hubert
Sako, Masao
Smith, Mathew
Zheng, Chen
Nichol, Robert C.
Bassett, Bruce
Bender, Ralf
Depoy, Darren L.
Doi, Mamoru
Elson, Ed
Filippenko, Alexei V.
Foley, Ryan J.
Garnavich, Peter M.
Hopp, Ulrich
Ihara, Yutaka
Ketzeback, William
Kollatschny, W.
Konishi, Kohki
Marshall, Jennifer L.
McMillan, Russet J.
Miknaitis, Gajus
Morokuma, Tomoki
Mortsell, Edvard
Pan, Kaike
Prieto, Jose Luis
Richmond, Michael W.
Riess, Adam G.
Romani, Roger
Schneider, Donald P.
Sollerman, Jesper
Takanashi, Naohiro
Tokita, Kouichi
van der Heyden, Kurt
Wheeler, J. C.
Yasuda, Naoki
York, Donald
TI FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II SUPERNOVA RESULTS: HUBBLE DIAGRAM
AND COSMOLOGICAL PARAMETERS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmological parameters; cosmology: observations; distance scale;
methods: data analysis; supernovae: general; surveys
ID SOUTHERN SPECTROPHOTOMETRIC STANDARDS; HIGH-REDSHIFT SUPERNOVAE; IA
SUPERNOVAE; DARK ENERGY; SPACE-TELESCOPE; ACCELERATING UNIVERSE;
EXTINCTION CURVES; LEGACY SURVEY; K-CORRECTIONS; DATA RELEASE
AB We present measurements of the Hubble diagram for 103 Type Ia supernovae (SNe) with redshifts 0.04 < z < 0.42, discovered during the first season (Fall 2005) of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. These data fill in the redshift "desert" between low-and high-redshift SN Ia surveys. Within the framework of the MLCS2K2 light-curve fitting method, we use the SDSS-II SN sample to infer the mean reddening parameter for host galaxies, R(V) = 2.18 +/- 0.14(stat) +/- 0.48(syst), and find that the intrinsic distribution of host-galaxy extinction is well fitted by an exponential function, P(Lambda(V)) = exp(-Lambda(V)/tau(V)), with tau(V) = 0.334 +/- 0.088 mag. We combine the SDSS-II measurements with new distance estimates for published SN data from the ESSENCE survey, the Supernova Legacy Survey (SNLS), the Hubble Space Telescope (HST), and a compilation of Nearby SN Ia measurements. A new feature in our analysis is the use of detailed Monte Carlo simulations of all surveys to account for selection biases, including those from spectroscopic targeting. Combining the SN Hubble diagram with measurements of baryon acoustic oscillations from the SDSS Luminous Red Galaxy sample and with cosmic microwave background temperature anisotropy measurements from the Wilkinson Microwave Anisotropy Probe, we estimate the cosmological parameters w and Omega M, assuming a spatially flat cosmological model (FwCDM) with constant dark energy equation of state parameter, w. We also consider constraints upon Omega(M) and Omega(A) for a cosmological constant model (Lambda CDM) with w = -1 and non-zero spatial curvature. For the FwCDM model and the combined sample of 288 SNe Ia, we find w = -0.76 +/- 0.07(stat)+/- 0.11(syst), Omega(M) = 0.307+/-0.019(stat)+/-0.023(syst) using MLCS2K2 and w = -0.96 +/- 0.06(stat) +/- 0.12(syst), Omega(M) = 0.265 +/- 0.016(stat) +/- 0.025(syst) using the SALT-II fitter. We trace the discrepancy between these results to a difference in the rest-frame UV model combined with a different luminosity correction from color variations; these differences mostly affect the distance estimates for the SNLS and HST SNe. We present detailed discussions of systematic errors for both light-curve methods and find that they both show data-model discrepancies in rest-frame U band. For the SALT-II approach, we also see strong evidence for redshift-dependence of the color-luminosity parameter (beta). Restricting the analysis to the 136 SNe Ia in the Nearby+SDSS-II samples, we find much better agreement between the two analysis methods but with larger uncertainties: w = -0.92 +/- 0.13(stat)(-0.33)(+0.10)(syst) for MLCS2K2 and w = -0.92 +/- 0.11(stat)(-0.15)(+0.07) (syst) for SALT-II.
C1 [Kessler, Richard; Frieman, Joshua A.; York, Donald] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Kessler, Richard; Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Becker, Andrew C.; Vanderplas, Jake] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Cinabro, David] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48202 USA.
[Frieman, Joshua A.; Marriner, John; Miknaitis, Gajus] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Davis, Tamara M.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Davis, Tamara M.; Sollerman, Jesper] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Dilday, Benjamin; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Lampeitl, Hubert; Smith, Mathew; Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Smith, Mathew; Bassett, Bruce; Elson, Ed] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa.
[Zheng, Chen; Romani, Roger] Stanford Univ, Kavli Inst Particle Astrophys Cosmol, Stanford, CA 94305 USA.
[Bassett, Bruce] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Bender, Ralf; Hopp, Ulrich] Univ Munich, Univ Sternwarte, D-80539 Munich, Germany.
[Depoy, Darren L.; Marshall, Jennifer L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Doi, Mamoru; Ihara, Yutaka; Konishi, Kohki; Tokita, Kouichi] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Doi, Mamoru] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Filippenko, Alexei V.; Foley, Ryan J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Garnavich, Peter M.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Ihara, Yutaka; Tokita, Kouichi] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Ketzeback, William; McMillan, Russet J.; Pan, Kaike] Apache Point Observ, Sunspot, NM 88349 USA.
[Kollatschny, W.] Univ Gottingen, Dept Astron, D-37077 Gottingen, Germany.
[Miknaitis, Gajus] Ctr Neighborhood Technol, Chicago, IL 60647 USA.
[Morokuma, Tomoki; Takanashi, Naohiro] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Mortsell, Edvard] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Prieto, Jose Luis] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Richmond, Michael W.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
[Riess, Adam G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Wheeler, J. C.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Yasuda, Naoki] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan.
[York, Donald] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
RP Kessler, R (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kessler@kicp.uchicago.edu
RI Yasuda, Naoki/A-4355-2011; Davis, Tamara/A-4280-2008;
OI Davis, Tamara/0000-0002-4213-8783; Sollerman, Jesper/0000-0003-1546-6615
FU JSPS Fellowship; NSF [AST-0607485]; DOE [DE-FG02-08ER41563]; Alfred P.
Sloan Foundation; Participating Institutions; National Science
Foundation; U.S. Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England
FX All software used in this analysis is publicly available from our Web
site (Kessler et al. 2009). We wish to thank J. Guy for retraining the
SALT-II program and for consulting on its use and results. We thank
Armin Rest for modifying the ESSENCE SN-search pipeline for use in the
SDSS SN survey. We gratefully acknowledge support from the Kavli
Institute for Cosmological Physics at the University of Chicago, the
National Science Foundation atWayne State, the Japan Society for the
Promotion of Science (JSPS), and the Department of Energy at Fermilab,
the University of Chicago, and Rutgers University. R. J. F. is supported
by a Clay Fellowship. Y. Ihara and T. Morokuma are supported by a JSPS
Fellowship. A. V. F. is grateful for the support of NSF grant
AST-0607485 and DOE grant DE-FG02-08ER41563. Funding for the creation
and distribution of the SDSS and SDSS-II has been provided by the Alfred
P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, the U.S. Department of Energy, the National
Aeronautics and Space Administration, the Japanese Monbukagakusho, the
Max Planck Society, and the Higher Education Funding Council for
England. The SDSS Web site is http://www.sdss.org/.
NR 91
TC 416
Z9 420
U1 4
U2 29
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2009
VL 185
IS 1
BP 32
EP 84
DI 10.1088/0067-0049/185/1/32
PG 53
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514NZ
UT WOS:000271402900003
ER
PT J
AU Krick, JE
Surace, JA
Thompson, D
Ashby, MLN
Hora, J
Gorjian, V
Yan, L
Frayer, DT
Egami, E
Lacy, M
AF Krick, J. E.
Surace, J. A.
Thompson, D.
Ashby, M. L. N.
Hora, J.
Gorjian, V.
Yan, L.
Frayer, D. T.
Egami, E.
Lacy, M.
TI THE INFRARED ARRAY CAMERA DARK FIELD: FAR-INFRARED TO X-RAY DATA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: photometry
ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; MULTIBAND IMAGING
PHOTOMETER; ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; IRAC SHALLOW
SURVEY; HUBBLE DEEP FIELD; 160 MU-M; ABSOLUTE CALIBRATION; STELLAR
POPULATIONS
AB We present 20 band photometry from the far-IR to X-ray in the Spitzer Infrared Array Camera ( IRAC) dark field. The bias for the near-IR camera on Spitzer is calibrated by observing a similar to 20' diameter "dark" field near the north ecliptic pole roughly every two-to-three weeks throughout the mission duration of Spitzer. The field is unique for its extreme depth, low background, high quality imaging, time-series information, and accompanying photometry including data taken with Akari, Palomar, MMT, KPNO, Hubble, and Chandra. This serendipitous survey contains the deepest mid-IR data taken to date. This data set is well suited for studies of intermediate-redshift galaxy clusters, high-redshift galaxies, the first generation of stars, and the lowest mass brown dwarfs, among others. This paper provides a summary of the data characteristics and catalog generation from all bands collected to date as well as a discussion of photometric redshifts and initial and expected science results and goals. To illustrate the scientific potential of this unique data set, we also present here IRAC color-color diagrams.
C1 [Krick, J. E.; Surace, J. A.; Yan, L.; Lacy, M.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
[Ashby, M. L. N.; Hora, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Frayer, D. T.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91109 USA.
[Egami, E.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
RP Krick, JE (reprint author), CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
EM jkrick@caltech.edu
OI Hora, Joseph/0000-0002-5599-4650
FU NASA through a grant from the Space Telescope Science Institute [10521,
NAS 5-26555]; NSF [AST97-31180]; Kitt Peak National Observatory;
National Aeronautics and Space Administration through Chandra Award
[G07-8120, NAS8-03060]
FX We thank the anonymous referee for useful suggestions on the manuscript.
This research has made use of data from the Two Micron All Sky Survey,
which is a joint project of the University of Massachusetts and the
Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This work was based on observations
obtained with the Hale Telescope, Palomar Observatory as part of a
continuing collaboration between the California Institute of Technology,
NASA/JPL, and Cornell University, the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA, and the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc. Support for program # 10521 was provided by NASA through a grant
from the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555. FLAMINGOS was designed and constructed by the IR
instrumentation group (PI: R. Elston) at the University of Florida,
Department of Astronomy, with support from NSF grant AST97-31180 and
Kitt Peak National Observatory. Observations reported here were obtained
at the MMT Observatory, a joint facility of the Smithsonian Institution
and theUniversity of Arizona. Support for this work was provided by the
National Aeronautics and Space Administration through Chandra Award
Number G07-8120 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.
NR 55
TC 7
Z9 7
U1 0
U2 1
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 NOV
PY 2009
VL 185
IS 1
BP 85
EP 97
DI 10.1088/0067-0049/185/1/85
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514NZ
UT WOS:000271402900004
ER
PT J
AU Tothill, NFH
Lohr, A
Parshley, SC
Stark, AA
Lane, AP
Harnett, JI
Wright, GA
Walker, CK
Bourke, TL
Myers, PC
AF Tothill, N. F. H.
Loehr, A.
Parshley, S. C.
Stark, A. A.
Lane, A. P.
Harnett, J. I.
Wright, G. A.
Walker, C. K.
Bourke, T. L.
Myers, P. C.
TI LARGE-SCALE CO MAPS OF THE LUPUS MOLECULAR CLOUD COMPLEX
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: clouds; ISM: individual (Lupus); submillimeter
ID C-12/C-13 ISOTOPE RATIO; MASS STAR-FORMATION; SPITZER C2D SURVEY; SMALL
DARK CLOUDS; DENSE CORES; GLOBULAR FILAMENTS; J=1-0 OBSERVATIONS; VISUAL
EXTINCTION; CORONA AUSTRALIS; BROWN DWARFS
AB Fully sampled degree-scale maps of the (13)CO 2-1 and CO 4-3 transitions toward three members of the Lupus Molecular Cloud Complex-Lupus I, III, and IV-trace the column density and temperature of the molecular gas. Comparison with IR extinction maps from the c2d project requires most of the gas to have a temperature of 8-10 K. Estimates of the cloud mass from (13)CO emission are roughly consistent with most previous estimates, while the line widths are higher, around 2 km s(-1). CO 4-3 emission is found throughout Lupus I, indicating widespread dense gas, and toward Lupus III and IV. Enhanced line widths at the NW end and along the edge of the B 228 ridge in Lupus I, and a coherent velocity gradient across the ridge, are consistent with interaction between the molecular cloud and an expanding H I shell from the Upper-Scorpius subgroup of the Sco-Cen OB Association. Lupus III is dominated by the effects of two HAe/Be stars, and shows no sign of external influence. Slightly warmer gas around the core of Lupus IV and a low line width suggest heating by the Upper-Centaurus-Lupus subgroup of Sco-Cen, without the effects of an H I shell.
C1 [Tothill, N. F. H.; Loehr, A.; Stark, A. A.; Lane, A. P.; Harnett, J. I.; Bourke, T. L.; Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tothill, N. F. H.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Parshley, S. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Harnett, J. I.] Natl Radio Astron Observ, Green Bank, WV USA.
[Wright, G. A.] Antiope Associates, Fair Haven, NJ 07704 USA.
[Walker, C. K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Tothill, NFH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nfht@astro.ex.ac.uk
RI Tothill, Nicholas/M-6379-2016
OI Tothill, Nicholas/0000-0002-9931-5162
FU National Science Foundation [OPP ANT-0441756]; University of Exeter
DVC(Resources) Discretionary Fund; European Commission
[MIRG-CT-2006-044961]
FX We thank Neal Evans, Fernando Comeron, Bruno Merin, Eric Mamajek, and
Tracy Huard for valuable discussions, and the many people who helped get
AST/RO ready for the 2005 observing season, particularly Jacob Kooi and
Craig Kulesa. Christina Hammock kept the liquid helium flowing through
the winter. We thank her, and all the South Pole Station staff, for
their work. We thank the anonymous referee, whose comments have improved
this work. AST/RO was supported by the National Science Foundation,
under NSF OPP ANT-0441756. N. F. H. T. was also supported by the
University of Exeter DVC(Resources) Discretionary Fund and by the
European Commission (grant MIRG-CT-2006-044961). This work has made use
of NASA's Astrophysics Data System; the SIMBAD database operated at CDS,
Strasbourg; and the Skyview facility at NASA's Goddard Space Flight
Center.
NR 56
TC 12
Z9 12
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2009
VL 185
IS 1
BP 98
EP 123
DI 10.1088/0067-0049/185/1/98
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514NZ
UT WOS:000271402900005
ER
PT J
AU Kirk, JM
Ward-Thompson, D
Di Francesco, J
Bourke, TL
Evans, NJ
Merin, B
Allen, LE
Cieza, LA
Dunham, MM
Harvey, P
Huard, T
Jorgensen, JK
Miller, JF
Noriega-Crespo, A
Peterson, D
Ray, TP
Rebull, LM
AF Kirk, Jason M.
Ward-Thompson, Derek
Di Francesco, James
Bourke, Tyler L.
Evans, Neal J., II
Merin, Bruno
Allen, Lori E.
Cieza, Lucas A.
Dunham, Michael M.
Harvey, Paul
Huard, Tracy
Jorgensen, Jes K.
Miller, Jennifer F.
Noriega-Crespo, Alberto
Peterson, Dawn
Ray, Tom P.
Rebull, Luisa M.
TI THE SPITZER SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. II. THE
CEPHEUS FLARE OBSERVED WITH IRAC AND MIPS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Review
DE infrared: general; ISM: individual (Cepheus Flare); stars: formation
ID YOUNG STELLAR OBJECTS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS;
INFRARED ARRAY CAMERA; MAIN-SEQUENCE STARS; CLERK MAXWELL TELESCOPE;
HERBIG AE/BE STARS; C2D SMALL CLOUDS; ALL-SKY SURVEY; MOLECULAR CLOUDS
AB We present Spitzer Infrared Array Camera (IRAC; similar to 2 deg(2)) and Multiband Imaging Photometer for Spitzer (MIPS; similar to 8 deg(2)) observations of the Cepheus Flare, which is associated with the Gould Belt, at an approximate distance of similar to 300 pc. Around 6500 sources are detected in all four IRAC bands, of which similar to 900 have MIPS 24 mu m detections. We identify 133 young stellar object (YSO) candidates using color-magnitude diagram techniques, and a large number of the YSO candidates are associated with the NGC 7023 reflection nebula. Cross-identifications were made with the Guide Star Catalog II and the IRAS Faint Source Catalog, and spectral energy distributions (SEDs) were constructed. SED modeling was conducted to estimate the degree of infrared excess. It was found that a large majority of disks were optically thick accreting disks, suggesting that there has been little disk evolution in these sources. Nearest neighbor clustering analysis identified four small protostellar groups (L1228, L1228N, L1251A, and L1251B) with 5-15 members each and the larger NGC 7023 association with 32 YSO members. The star-formation efficiency for cores with clusters of protostars and for those without clusters was found to be similar to 8% and similar to 1%, respectively. The cores L1155, L1241, and L1247 are confirmed to be starless down to our luminosity limit of L-bol = 0.06 L-circle dot.
C1 [Kirk, Jason M.; Ward-Thompson, Derek] Cardiff Univ, Sch Phys & Astron, Cardiff CF2 3AA, S Glam, Wales.
[Di Francesco, James] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Bourke, Tyler L.; Allen, Lori E.; Peterson, Dawn] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Evans, Neal J., II; Dunham, Michael M.; Harvey, Paul] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Merin, Bruno] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Cieza, Lucas A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Huard, Tracy; Miller, Jennifer F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Noriega-Crespo, Alberto; Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Ray, Tom P.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
RP Kirk, JM (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF2 3AA, S Glam, Wales.
EM jason.kirk@astro.cf.ac.uk; derek.ward-thompson@astro.cf.ac.uk;
james.difrancesco@nrc-cnrc.gc.ca; bourke@cfa.harvard.edu;
nje@bubba.as.utexas.edu; Bruno.Merin@sciops.esa.int;
leallen@cfa.harvard.edu; lcieza@ifa.hawaii.edu;
mdunham@astro.as.utexas.edu; pmh@astro.as.utexas.edu;
thuard@astro.umd.edu; jes@astro.uni-bonn.de; jfm@astro.umd.edu;
alberto@ipac.caltech.edu; dpeterson@cfa.harvard.edu; tr@cp.dias.ie;
rebull@ipac.caltech.edu
OI Rebull, Luisa/0000-0001-6381-515X; Merin, Bruno/0000-0002-8555-3012
NR 152
TC 41
Z9 41
U1 0
U2 6
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 NOV
PY 2009
VL 185
IS 1
BP 198
EP 249
DI 10.1088/0067-0049/185/1/198
PG 52
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514NZ
UT WOS:000271402900010
ER
PT J
AU Young, M
Elvis, M
Risaliti, G
AF Young, M.
Elvis, M.
Risaliti, G.
TI THE FIFTH DATA RELEASE SLOAN DIGITAL SKY SURVEY/XMM-NEWTON QUASAR SURVEY
(vol 183, pg 17, 2009)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Correction
C1 [Young, M.; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Young, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
RP Young, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM myoung@cfa.harvard.edu
NR 1
TC 2
Z9 2
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2009
VL 185
IS 1
BP 250
EP 251
DI 10.1088/0067-0049/185/1/250
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514NZ
UT WOS:000271402900011
ER
PT J
AU Baugh, AT
Ryan, MJ
AF Baugh, Alexander T.
Ryan, Michael J.
TI Female tungara frogs vary in commitment to mate choice
SO BEHAVIORAL ECOLOGY
LA English
DT Article
DE body condition; choosiness; dynamic behavior; individual differences;
mate choice; phonotaxis
ID PHYSALAEMUS-PUSTULOSUS; MATING PREFERENCES; SEXUAL SELECTION; BODY
CONDITION; HYPEROLIUS-MARMORATUS; REED FROG; SIZE; SIGNALS;
ADVERTISEMENT; RESIDUALS
AB Mate choice studies most often examine female preferences based on population responses, thus potentially overlooking individual differences in behavior. Moreover, such studies typically use invariant stimulus conditions to infer preferences. By using population responses and static stimulus presentations, it is difficult to thoroughly understand the complexity of the mate choice process, including variation present between individuals. Here, we investigated phonotactic mate choice behavior in female tungara frogs (Physalaemus pustulosus) in response to temporally dynamic presentations of male advertisement calls. We tested females on repeated trials to examine individual differences and found considerable variation in the extent to which females update their mate choice decisions. Females in our study were bimodally distributed and thus broadly classified as either committed or uncommitted to an initial mate approach. We compared body condition measures of females differing behaviorally and determined that females with larger residual body masses were more committed to initial mate choices than less massive individuals, despite the fact that all females were in reproductive condition and field collected in amplexus. Our results suggest that anuran phonotaxis, once considered to be a highly stereotyped behavior, is more complex and variable than previously thought.
C1 [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Inst Neurosci, Austin, TX 78712 USA.
[Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
RP Baugh, AT (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn,C0930, Austin, TX 78712 USA.
EM alex.baugh@gmail.com
RI Baugh, Alexander/E-4777-2010;
OI Baugh, Alexander/0000-0003-2032-892X
FU University of Texas at Austin; National Science Foundation [IOB 0544096]
FX Homer Lindsay Bruce Endowed Fellowship at The University of Texas at
Austin ( to A. T. Baugh) and National Science Foundation (IOB 0544096 to
M.J. Ryan).
NR 44
TC 14
Z9 14
U1 0
U2 9
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
J9 BEHAV ECOL
JI Behav. Ecol.
PD NOV-DEC
PY 2009
VL 20
IS 6
BP 1153
EP 1159
DI 10.1093/beheco/arp120
PG 7
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA 520BB
UT WOS:000271813600001
ER
PT J
AU Aisenberg, A
Eberhard, WG
AF Aisenberg, Anita
Eberhard, William G.
TI Female cooperation in plug formation in a spider: effects of male
copulatory courtship
SO BEHAVIORAL ECOLOGY
LA English
DT Article
DE copulatory courtship; copulatory plug; cryptic female choice; sexual
selection
ID SEXUAL CONFLICT; WATER STRIDERS; BEHAVIOR; ARANEAE; CHOICE; INSECTS;
MORPHOLOGY; BEETLES; SUCCESS; PATTERN
AB One of the strongest indications that cryptic female choice is an evolutionary phenomenon of general importance is the widespread existence of male courtship behavior during copulation. It has been presumed that such copulatory courtship functions to induce female reproductive behavior that favors the male's reproductive interests, but this function has seldom been demonstrated. Here, we examine the possible effects of male copulatory courtship in the spider Leucauge mariana (Tetragnathidae) on whether a female will aid the male in forming a copulatory plug, thus reducing the chances that future mates will be able to inseminate her. Greater numbers of 2 behavior patterns by the male during copulation, rhythmic pushing on the female's legs with his front legs, and repeated short insertions with his genitalia were associated with increased chances that the female would cooperate in plug formation. This confirms that these behavior patterns do indeed function as courtship.
C1 [Aisenberg, Anita] Inst Invest Biol Clemente Estable, Lab Etol Ecol & Evoluc, Montevideo 11600, Uruguay.
[Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica.
[Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica.
RP Aisenberg, A (reprint author), Inst Invest Biol Clemente Estable, Lab Etol Ecol & Evoluc, Ave Italia 3318, Montevideo 11600, Uruguay.
EM aisenber@iibce.edu.uy
NR 33
TC 23
Z9 25
U1 0
U2 12
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
J9 BEHAV ECOL
JI Behav. Ecol.
PD NOV-DEC
PY 2009
VL 20
IS 6
BP 1236
EP 1241
DI 10.1093/beheco/arp117
PG 6
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA 520BB
UT WOS:000271813600012
ER
PT J
AU Giorgi, JA
Vandenberg, NJ
McHugh, JV
Forrester, JA
Silpinski, SA
Miller, KB
Shapiro, LR
Whiting, MF
AF Giorgi, Jose Adriano
Vandenberg, Natalia J.
McHugh, Joseph V.
Forrester, Juanita A.
Silpinski, S. Adam
Miller, Kelly B.
Shapiro, Lori R.
Whiting, Michael F.
TI The evolution of food preferences in Coccinellidae
SO BIOLOGICAL CONTROL
LA English
DT Review
DE Lady beetles; Ladybirds; Ladybugs; Food preference; Prey; Evolution;
Trophic shifts; Phylogeny; Coleoptera; Coccinellidae; Cerylonid Series;
Cucujoidea
ID COLEOMEGILLA-MACULATA COLEOPTERA; HARMONIA-AXYRIDIS COLEOPTERA;
ENDOMYCHIDAE COLEOPTERA; MULSANT COLEOPTERA; BIOLOGICAL-CONTROL;
HIEROGLYPHICA COL; LADYBIRD BEETLES; NATURAL ENEMIES; PHYLOGENY;
HEMIPTERA
AB Despite the familiarity and economic significance of Coccinellidae, the family has thus far escaped analysis by rigorous phylogenetic methods. As a result, the internal classification remains unstable and there is no framework with which to interpret evolutionary events within the family. Coccinellids exhibit a wide range of preferred food types spanning kingdoms, and trophic levels. To provide an evolutionary perspective on coccinellid feeding preferences, we performed a phylogenetic analysis of 62 taxa based on the ribosomal nuclear genes 18S and 28S. The entire dataset consists of 3957 aligned nucleotide sites, 787 of which are parsimony informative. Bayesian and parsimony analyses were performed. Host preferences were mapped onto the Bayesian tree to infer food preference transitions. Our results indicate that the ancestral feeding condition for Coccinellidae is coccidophagy. From the ancestral condition, there have been at least three transitions to aphidophagy and one transition to leaf-eating phytophagy. A second transition to leaf-eating phytophagy arose within an aphidophagous/pollinivorous clade. The mycophagous condition in Halyziini originated from aphidophagy. Our findings suggest that polyphagy served as an evolutionary stepping stone for primarily predaceous groups to adopt new feeding habits. The analyses recovered a clade comprising Serangiini plus Microweiseini as the sister group to the rest of Coccinellidae. The subfamilies Coccinellinae and Epilachninae are monophyletic; however, Sticholotidinae, Chilocorinae, Scymninae, and Coccidulinae are paraphyletic. Our results do not support the traditional view of phylogenetic relationships among the coccinellid subfamilies. These results indicate that the current classification system poorly reflects the evolution of Coccinellidae and therefore requires revision. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Giorgi, Jose Adriano; McHugh, Joseph V.; Forrester, Juanita A.] Univ Georgia, Dept Entomol, Athens, GA 30602 USA.
[Vandenberg, Natalia J.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
[Silpinski, S. Adam] CSIRO Entomol, Canberra, ACT 2601, Australia.
[Miller, Kelly B.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Shapiro, Lori R.] Penn State Univ, Dept Entomol, University Pk, PA 16802 USA.
[Whiting, Michael F.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA.
[Whiting, Michael F.] Brigham Young Univ, ML Bean Life Sci Museum, Provo, UT 84602 USA.
RP Giorgi, JA (reprint author), Univ Georgia, Dept Entomol, 413 Biol Sci Bldg, Athens, GA 30602 USA.
EM coccinellid@gmail.com
RI Slipinski, Stanislaw Adam/B-4293-2009; Miller, Kelly/I-6651-2012;
McHugh, Joseph/P-7417-2015
OI McHugh, Joseph/0000-0002-7954-6254
FU N.S.F [DEB-0329115, EF-0531665]
FX This work was supported by N.S.F. PEET Grant DEB-0329115 (to J.V.M.,
K.B.M., and M.F.W.) and N.S.F. AToL Grant EF-0531665 (to M.F.W. and
subcontract to J.V.M.). Additional support was provided by the
Department of Entomology and the H.H. Ross Memorial Fund at The
University of Georgia. The senior author thanks all members of the
McHugh Lab and Whiting Lab for their assistance with various phases of
the project.
NR 142
TC 56
Z9 61
U1 3
U2 38
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1049-9644
EI 1090-2112
J9 BIOL CONTROL
JI Biol. Control
PD NOV
PY 2009
VL 51
IS 2
SI SI
BP 215
EP 231
DI 10.1016/j.biocontrol.2009.05.019
PG 17
WC Biotechnology & Applied Microbiology; Entomology
SC Biotechnology & Applied Microbiology; Entomology
GA 505LW
UT WOS:000270696000002
ER
PT J
AU Oprea, M
Esberard, CEL
Weira, TB
Mendes, P
Pimenta, VT
Brito, D
Ditchfield, AD
AF Oprea, M.
Esberard, C. E. L.
Weira, T. B.
Mendes, P.
Pimenta, V. T.
Brito, D.
Ditchfield, A. D.
TI Bat community species richness and composition in a restinga protected
area in Southeastern Brazil
SO BRAZILIAN JOURNAL OF BIOLOGY
LA English
DT Article
DE Chiroptera; community ecology; diversity; restinga
ID DE-JANEIRO STATE; ATLANTIC FOREST
AB In Brazil, restingas are under severe human-induced impacts resulting in habitat degradation and loss and remain one of the less frequently studied ecosystems. The main objectives of the present study are to describe the bat community in a restinga in Paulo Cesar Vinha State Park, Guarapari municipality, state of Espirito Santo, southeastern Brazil. Fieldwork was conducted twice a month from August 2004 to September 2005. A total sampling effort of 40,300 m(2)/h, represents the largest sampling effort for sampling bats in restingas to date. Bats were sampled in five different vegetational types in the area. Captured bats were processed recording information on species, sex, age, forearm length and weight. Shannon Diversity and Jaccard indexes were used to analyse diversity and similarity among habitats in the Park. A total of 554 captures belonging to 14 species and two families were obtained. Noctilio leporinus was recorded through direct observation and an ultra-sound detector also registered the presence of individuals from the family Molossidae, without being possible to distinguish it at specific level. Frugivores were the most representative guild. Richness was higher in Clusia shrubs (I I species) and Carais lagoon (10 species). Shannon diversity index was estimated at H' = 1.43 for the overall sample, with Carais lagoon representing the most diverse habitat (H' = 1.60). The greater similarity (J = 0.714) was observed for the two areas under high human influence.
C1 [Oprea, M.; Weira, T. B.; Mendes, P.; Pimenta, V. T.; Ditchfield, A. D.] Univ Fed Espirito Santo, Lab Estudos Quiropteros, Dept Ciencias Biol, BR-29040090 Vitoria, ES, Brazil.
[Oprea, M.] Smithsonian Inst, Natl Museum Nat Hist, MRC 108, Div Mammals, Washington, DC 20013 USA.
[Esberard, C. E. L.] UFRRJ, Inst Biol, Lab Diversidade Morcegos, BR-23890000 Seropedica, RJ, Brazil.
[Brito, D.] Ctr Appl Biodivers Sci, Arlington, VA 22202 USA.
[Brito, D.] Univ Fed Amapa UNIFAP, Programa Posgrad Biodiversidade Trop, BR-68902280 Macapa, AP, Brazil.
RP Oprea, M (reprint author), Univ Fed Espirito Santo, Lab Estudos Quiropteros, Dept Ciencias Biol, Av Marechal Campos 1468, BR-29040090 Vitoria, ES, Brazil.
EM monik.bats@gmail.com
RI Oprea, Monik/E-6204-2010; Brito, Daniel/A-4014-2008; Esberard,
carlos/A-2493-2013
OI Brito, Daniel/0000-0003-1131-4622;
NR 41
TC 8
Z9 9
U1 0
U2 23
PU INT INST ECOLOGY
PI SAO CARLOS
PA RUA BENTO CARLOS, 750 - CENTRO, SAO CARLOS, SP 00000, BRAZIL
SN 1519-6984
J9 BRAZ J BIOL
JI Braz. J. Biol.
PD NOV
PY 2009
VL 69
IS 4
BP 1073
EP 1079
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 518FA
UT WOS:000271674700009
PM 19967177
ER
PT J
AU Kaltenegger, L
Selsis, F
AF Kaltenegger, Lisa
Selsis, Franck
TI Characterizing habitable extrasolar planets using spectral fingerprints
SO COMPTES RENDUS PALEVOL
LA English
DT Article
DE Habitable planets; Extrasolar planet search; Biomarkers; Planetary
atmospheres
ID EARTH-LIKE PLANETS; TERRESTRIAL PLANETS; INFRARED RADIATION; THERMAL
EMISSION; SOLAR PLANETS; HD 189733B; RED-EDGE; SEARCH; LIFE; ATMOSPHERE
AB The detection and characterization of an Earth-like planet is approaching rapidly thanks to radial velocity (RV) surveys (e.g. HARPS) and transit searches (Corot, Kepler). A rough characterization of these planets will be already achievable in 2014 with the James Webb Space Telescope, and more detailed spectral studies will be obtained by future large ground based telescopes (ELT, TNT, GMT), and dedicated space-based missions like Darwin, Terrestrial Planet Finder, New World Observer. In this article we discuss how we can read a planet's spectrum to assess its habitability and search for the signatures of a biosphere. Identifying signs of fife implies understanding how the observed atmosphere physically and chemically works, and thus gathering information on the planet in addition to observing its spectral fingerprint. To cite this article: L. Kaltenegger, F Selsis, C. R. Palevol 8 (2009). (C) 2009 Published by Elsevier Masson SAS on behalf of l'Academie des sciences.
C1 [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Selsis, Franck] Univ Bordeaux 1, CNRS, Lab Astrophys Bordeaux, F-33271 Floirac, France.
RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM lkaltenegger@cfa.harvard.edu; selsis@obs.u-bordeaux1.fr
FU Harvard Origins of Life Initiative; NASA Astrobiology Institute
FX L. Kaltenegger acknowledges the support of the Harvard Origins of Life
Initiative and the NASA Astrobiology Institute.
NR 68
TC 3
Z9 3
U1 2
U2 6
PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75724 PARIS, FRANCE
SN 1631-0683
J9 CR PALEVOL
JI C. R. Palevol
PD NOV
PY 2009
VL 8
IS 7
BP 679
EP 691
DI 10.1016/j.crpv.2009.07.001
PG 13
WC Paleontology
SC Paleontology
GA 539QI
UT WOS:000273271900008
ER
PT J
AU Cardoso, P
Borges, PAV
Veech, JA
AF Cardoso, Pedro
Borges, Paulo A. V.
Veech, Joseph A.
TI Testing the performance of beta diversity measures based on incidence
data: the robustness to undersampling
SO DIVERSITY AND DISTRIBUTIONS
LA English
DT Article
DE Accumulation curves; arthropods; beta diversity; completeness; sampling;
similarity indices
ID PRESENCE-ABSENCE DATA; SPECIES RICHNESS; BIODIVERSITY ASSESSMENT;
SIMILARITY INDEXES; SPATIAL TURNOVER; DISTANCE-DECAY; COMMUNITIES;
FORESTS; BIAS; ARTHROPODS
AB Aim
Researchers measuring beta diversity have rarely concerned themselves with the problems of how complete the species lists of studied communities are, and of how the varying degrees of completeness can actually change estimates of beta diversity. No comprehensive assessment has been made regarding the behaviour of most beta diversity indices when applied to incomplete samples, a situation which is more common than usually recognized. Our objective was to assess the behaviour and robustness of a number of beta diversity measures for incidence data from undersampled communities.
Location
Mainland Portugal and the Azorean archipelago (North Atlantic).
Methods
Data from intensive sampling of spiders in mainland Portugal and arthropods in Azores were collected. We examined the properties of 15 beta diversity measures developed for incidence data. We simulated varying degrees of completeness, whereas computing beta diversity for selected pairs of samples. The robustness of these beta diversity accumulation curves was assessed for the purpose of finding the best measures for undersampled communities.
Results
The Harrison et al.beta(-2) and the Williams beta(-3) are particularly robust to undersampling. These measures are also insensitive to differences of alpha diversity (species richness) between communities, and therefore to nestedness. Colwell & Coddington beta(cc) and the related Jaccard beta(j) and Gaston et al.beta(g) performed best of the measures sensitive to alpha diversity. They performed poorly, however, when compared communities exhibited very low values of beta diversity. In such cases, the Routledge beta(r) performed the best.
Main conclusions
No index was found to perform without bias in all circumstances. Overall, beta(-2), beta(-3) and beta(cc) (or related measures beta(j) and beta(g)) are recommended as they seem to be the most robust to undersampling.
C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
[Cardoso, Pedro; Borges, Paulo A. V.] Univ Acores, Dep Ciencias Agr, CITA A, Azorean Biodivers Grp, Angra Do Heroismo, Portugal.
[Cardoso, Pedro] Univ Copenhagen, Zool Museum, Nat Hist Museum Denmark, DK-2100 Copenhagen, Denmark.
[Cardoso, Pedro] Univ Copenhagen, Ctr Macroecol, Copenhagen, Denmark.
[Veech, Joseph A.] Texas State Univ, Dept Biol, San Marcos, TX USA.
RP Cardoso, P (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 105,Room E-509, Washington, DC 20013 USA.
EM pcardoso@ennor.org
RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960
FU Fundacao para a Ciencia e Tecnologia [SFRH/BPD/17351/2004]; Direccao
Regional da Ciencia e Tecnologia dos Acores [M112/F/014/2007]; CITA-A
FX We express our gratitude to S. Ferrier, J. Hortal, K. Triantis, M.
Rodriguez and M. Almeida-Neto for valuable comments on previous versions
of the manuscript. Thanks to R. Meneses for the English revision. We
would also like to thank all the people that helped with the fieldwork,
both in mainland Portugal and the Azorean archipelago. PC was supported
by Fundacao para a Ciencia e Tecnologia (SFRH/BPD/17351/2004) and
Direccao Regional da Ciencia e Tecnologia dos Acores (M112/F/014/2007).
PAVB was funded by a grant from CITA-A.
NR 54
TC 35
Z9 35
U1 3
U2 26
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1366-9516
J9 DIVERS DISTRIB
JI Divers. Distrib.
PD NOV
PY 2009
VL 15
IS 6
BP 1081
EP 1090
DI 10.1111/j.1472-4642.2009.00607.x
PG 10
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 505XN
UT WOS:000270735000016
ER
PT J
AU McCormick, MK
Whigham, DF
O'Neill, JP
Becker, JJ
Werner, S
Rasmussen, HN
Bruns, TD
Taylor, DL
AF McCormick, Melissa K.
Whigham, Dennis F.
O'Neill, John P.
Becker, Janie J.
Werner, Sarah
Rasmussen, Hanne N.
Bruns, Thomas D.
Taylor, D. Lee
TI Abundance and distribution of Corallorhiza odontorhiza reflect
variations in climate and ectomycorrhizae
SO ECOLOGICAL MONOGRAPHS
LA English
DT Article
DE Corallorhiza odontorhiza; ECM; ectomycorrhiza; mycoheterotrophic;
orchid; Orchidaceae; Smithsonian Environmental Research Center;
Tomentella
ID MYCO-HETEROTROPHIC PLANTS; SYMBIOTIC GERMINATION; PREPACKAGED SYMBIOSES;
POPULATION-DYNAMICS; TERRESTRIAL ORCHIDS; FUNGAL COMMUNITIES; PROLONGED
DORMANCY; ECOLOGY; DIVERSITY; PATTERNS
AB The abundance and reproductive activity of orchids have been linked to variations in weather conditions, but few investigators have examined the relationships between orchid flowering dynamics and the distribution and abundance of mycorrhizal fungi. We quantified the abundance of flowering individuals of Corallorhiza odontorhiza, a mycoheterotrophic orchid, over a 14-year period and mapped the distribution of individuals in six of the 14 years. For two seasons, we conducted intensive and extensive studies of the mycorrhizal fungi that were associated with C. odontorhiza. The annual abundance of flowering plants was statistically related to growing-season precipitation and winter temperature, and the distribution of individuals within the study plot was related to the abundance and distribution of appropriate host fungi. We used DNA sequencing to identify ectomycorrhizal root tips that hosted Tomentella fungi that could potentially support C. odontorhiza. We found that Tomentella spp. were distributed throughout the study plot and on all ectomycorrhizal tree species, including in areas that have historically supported few or no orchids. However, there were fewer ectomycorrhizal trees, total ectomycorrhizal root tips, and root tips hosting Tomentella spp. in areas with few or no orchids compared to areas with abundant orchids. Furthermore, one Tomentella taxon dominated in C. odontorhiza rhizomes but was never found except immediately adjacent to C. odontorhiza plants. This suggests that abundance of flowering C. odontorhiza reflects both the presence of "preferred" taxa and abundance of appropriate host fungi associated with ectomycorrhizal roots. Results of this research provide the first indication that the relationship between plants and mycorrhizal fungi may be influenced by both the relative abundance of fungi that are sufficient to support orchid growth and by the presence of particular fungal types that are especially good at supporting orchid growth.
C1 [McCormick, Melissa K.; Whigham, Dennis F.; O'Neill, John P.; Becker, Janie J.; Werner, Sarah] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Rasmussen, Hanne N.] Univ Copenhagen, Danish Ctr Forest Landscape & Planning, DK-2970 Horsholm, Denmark.
[Bruns, Thomas D.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA.
[Taylor, D. Lee] Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA.
RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM mccormickm@si.edu
RI Rasmussen, Hanne/P-5485-2014;
OI Rasmussen, Hanne/0000-0002-0181-9304; Taylor,
Donald/0000-0002-5985-9210; Whigham, Dennis/0000-0003-1488-820X
FU Smithsonian Internship Program; Warren Wilson College; Smithsonian
Environmental Sciences Program; NSF [DEB-0316523]; Smithsonian-Mellon
Foundation; Smithsonian Scholarly Studies
FX The Smithsonian Internship Program supported work by J. J. Becker. S.
Werner was supported by an internship from Warren Wilson College. J. P.
O'Neill was funded by the Smithsonian Environmental Sciences Program.
This work was funded by NSF grant DEB-0316523 to D. F. Whigham, M. K.
McCormick, and D. L. Taylor; a Smithsonian-Mellon Foundation grant to T.
D. Bruns and D. F. Whigham; and a Smithsonian Scholarly Studies grant to
D. F. Whigham. The manuscript was improved by comments from two
anonymous reviewers.
NR 85
TC 33
Z9 35
U1 1
U2 18
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9615
EI 1557-7015
J9 ECOL MONOGR
JI Ecol. Monogr.
PD NOV
PY 2009
VL 79
IS 4
BP 619
EP 635
DI 10.1890/08-0729.1
PG 17
WC Ecology
SC Environmental Sciences & Ecology
GA 508ED
UT WOS:000270909900005
ER
PT J
AU Puebla, O
Bermingham, E
Guichard, F
AF Puebla, Oscar
Bermingham, Eldredge
Guichard, Frederic
TI Estimating dispersal from genetic isolation by distance in a coral reef
fish (Hypoplectrus puella)
SO ECOLOGY
LA English
DT Article
DE barred hamlet; connectivity; coral reef fishes; demography; dispersal;
Hypoplectrus puella; isolation by distance; marine; pelagic larvae;
population genetics; spatial scale
ID PACIFIC-OCEAN; POPULATION-STRUCTURE; LARVAL DISPERSAL; MARINE RESERVES;
F-STATISTICS; CONNECTIVITY; ROCKFISH; EASTERN; DIFFERENTIATION;
EQUILIBRIUM
AB The spatial scale of dispersal in coral reef fishes eludes ecologists despite the importance of this parameter for understanding the dynamics of ecological and evolutionary processes. Genetic isolation by distance (IBD) has been used to estimate dispersal in coral reef fishes, but its application in marine systems has been limited by insufficient sampling at different spatial scales and a lack of information regarding population density. Here, we present an analysis of IBD in the barred hamlet (Hypoplectrus puella, Serranidae) at spatial scales ranging from 10 to 3200 km complemented with SCUBA surveys of population densities covering 94 000 m(2) of reef. We used 10 hypervariable DNA markers to genotype 854 fish from 15 locations, and our results establish that IBD in H. puella emerges at a spatial scale of 175 km and is preserved up to the regional scale (3200 km). Assuming a normal or a Laplace dispersal function, our data are consistent with mean dispersal distances in H. puella that range between 2 and 14 km. Such small mean dispersal distances is a surprising result given the three-week pelagic larval duration of H. puella and the low level of genetic structure at the Caribbean scale (Wright's fixation index, F(ST), estimate = 0.005). Our data reinforce the importance of considering population density when estimating dispersal from IBD and underscore the relevance of sampling at local scales, even when genetic structure is weak at the regional scale.
C1 [Puebla, Oscar; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Puebla, Oscar; Bermingham, Eldredge; Guichard, Frederic] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
RP Puebla, O (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama.
EM oscar.puebla@mail.mcgill.ca
RI Guichard, Frederic/B-6188-2015
OI Guichard, Frederic/0000-0002-7369-482X
FU Smithsonian Marine Science Network; Levinson Family; Astroff-Buckshon
Family; McGill University; Natural Science and Engineering Research
Council of Canada
FX The authors thank the governments and authorities of Barbados, Belize,
Honduras, Panama, and Kuna Yala for research permits, and the R/V Urraca
and crew as well as the personnel of Carrie Bow Cay, Bocas del Toro, and
Bellairs research stations for support of our research. The Smithsonian
Marine Science Network provided financial support for our investigation,
and O. Puebla was supported by graduate fellowships from the Levinson
Family, the Astroff-Buckshon Family, and McGill University. F. Guichard
acknowledges support from the Natural Science and Engineering Research
Council of Canada. We are grateful to R. S. Waples and one anonymous
reviewer for insightful comments on an earlier version of the
manuscript. We also thank Jorge Andreve, Sandra Binning, Arcadio
Castillo, Owen McMillan, Edgardo Ochoa, Pablo Rico, and Dominique Roche
for help in the field.
NR 55
TC 32
Z9 32
U1 2
U2 34
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
J9 ECOLOGY
JI Ecology
PD NOV
PY 2009
VL 90
IS 11
BP 3087
EP 3098
DI 10.1890/08-0859.1
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 515GY
UT WOS:000271457300012
PM 19967864
ER
PT J
AU Myers, JA
Harms, KE
AF Myers, Jonathan A.
Harms, Kyle E.
TI Seed arrival, ecological filters, and plant species richness: a
meta-analysis
SO ECOLOGY LETTERS
LA English
DT Review
DE Community assembly; disturbance; immigration; propagule supply; seed
addition; seed dispersal; seed limitation; species coexistence; species
diversity; species pool
ID GRASSLAND PRODUCTIVITY GRADIENT; REGIONAL PROCESSES; COMMUNITY
DIVERSITY; RECRUITMENT LIMITATION; MICROSITE LIMITATION; ADDITION
EXPERIMENTS; PROPAGULE POOLS; RELATIVE ROLE; DISPERSAL; HISTORY
AB Theoretical models predict that effects of dispersal on local biodiversity are influenced by the size and composition of the species pool, as well as ecological filters that limit local species membership. We tested these predictions by conducting a meta-analysis of 28 studies encompassing 62 experiments examining effects of propagule supply (seed arrival) on plant species richness under contrasting intensities of ecological filters (owing to disturbance and resource availability). Seed arrival increased local species richness in a wide range of communities (forest, grassland, montane, savanna, wetland), resulting in a positive mean effect size across experiments. Mean effect size was 70% higher in disturbed relative to undisturbed communities, suggesting that disturbance increases recruitment opportunities for immigrating species. In contrast, effect size was not significantly influenced by nutrient or water availability. Among seed-addition experiments, effect size was positively correlated with species and functional diversity within the pool of added seeds (species evenness and seed-size diversity), primarily in disturbed communities. Our analysis provides experimental support for the general hypothesis that species pools and local environmental heterogeneity interactively structure plant communities. We highlight empirical gaps that can be addressed by future experiments and discuss implications for community assembly, species coexistence, and the maintenance of biodiversity.
C1 [Myers, Jonathan A.; Harms, Kyle E.] Louisiana State Univ, Div Systemat Ecol & Evolut, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Myers, JA (reprint author), Louisiana State Univ, Div Systemat Ecol & Evolut, Dept Biol Sci, Baton Rouge, LA 70803 USA.
EM jmyer19@lsu.edu
FU Torrey Botanical Society Graduate Student Fellowship; Sigma-Xi
Grant-In-Aid (Louisiana State University Chapter); Louisiana Office of
Environmental Education Grants; National Science Foundation
FX We thank Adriana Bravo, Jane Carlson, Jonathan Chase, Santiago
Claramunt, Jim Cronin, Paul Gagnon, Paul Keddy, Heather Jackson,
Jonathan Levine, David Johnson, Nicolas Mouquet, Tim Paine, Heather
Passmore, Bill Platt, Ellen Reid, Richard Stevens, and Sebastian Tello
for helpful comments throughout the course of the study. Jessica
Gurevitch and four anonymous referees provided many helpful comments on
the manuscript. We are grateful to the many authors that generously
provided supplementary data. Financial support was provided by a Torrey
Botanical Society Graduate Student Fellowship, Sigma-Xi Grant-In-Aid
(Louisiana State University Chapter), Louisiana Office of Environmental
Education Grants, and the National Science Foundation.
NR 79
TC 128
Z9 130
U1 15
U2 201
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD NOV
PY 2009
VL 12
IS 11
BP 1250
EP 1260
DI 10.1111/j.1461-0248.2009.01373.x
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 507CK
UT WOS:000270828100015
PM 19723285
ER
PT J
AU Adamski, D
LaGasa, EH
AF Adamski, David
LaGasa, Eric H.
TI DESCRIPTION OF LARVA, ADULTS, AND BIONOMICS OF FILATIMA DEMISSAE KEIFER
(LEPIDOPTERA: GELECHIIDAE) IN WASHINGTON, USA
SO ENTOMOLOGICAL NEWS
LA English
DT Article
DE chaetotaxy; Gelechiidae; Prunus; Purshia; Rosaceae; taxonomy
AB Descriptions of the adult, larva, and bionomics are based on larvae of Filatima demissae (Keifer) collected on Prunus virginiana L. and reared adults in Washington. Included are an image of the adult, illustrations of the male and female genitalia, and maps of the chaetotaxy of the last-instar, supplemented with scanning electron micrographs.
C1 [Adamski, David] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[LaGasa, Eric H.] Washington State Dept Agr, Olympia, WA 98504 USA.
RP Adamski, D (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,E-523, Washington, DC 20013 USA.
EM adamskid@si.edu; elagasa@agr.wa.gov
NR 13
TC 0
Z9 0
U1 1
U2 2
PU AMER ENTOMOL SOC
PI PHILADELPHIA
PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA
SN 0013-872X
EI 2162-3236
J9 ENTOMOL NEWS
JI Entomol. News
PD NOV-DEC
PY 2009
VL 120
IS 5
BP 453
EP 463
DI 10.3157/021.120.0501
PG 11
WC Entomology
SC Entomology
GA 695VL
UT WOS:000285400600001
ER
PT J
AU Nieuwenhuizen, TM
Gibson, CH
Schild, RE
AF Nieuwenhuizen, Th. M.
Gibson, C. H.
Schild, R. E.
TI Gravitational hydrodynamics of large-scale structure formation
SO EPL
LA English
DT Article
ID DARK-MATTER; MILKY-WAY; GALAXIES; UNIVERSE; NEBULA; CLOUDS; DUST; HALO
AB The gravitational hydrodynamics of the primordial plasma with neutrino hot dark matter is considered as a challenge to the bottom-up cold-dark-matter paradigm. Viscosity and turbulence induce a top-down fragmentation scenario before and at decoupling. The first step is the creation of voids in the plasma, which expand to 37 Mpc on the average now. The remaining matter clumps turn into galaxy clusters. At decoupling galaxies and Jeans clusters arise; the latter constitute the galactic dark-matter halos and consist themselves of earth mass milli brown dwarfs. Frozen milli brown dwarfs are observed in microlensing and white-dwarf-heated ones in planetary nebulae. The approach explains the Tully-Fisher and Faber-Jackson relations, and cosmic microwave background temperature fluctuations of sub-milli-kelvins. Copyright (C) EPLA, 2009
C1 [Nieuwenhuizen, Th. M.] Inst Theoret Phys, NL-1018 XE Amsterdam, Netherlands.
[Gibson, C. H.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
[Gibson, C. H.] Univ Calif San Diego, Scripps Inst Oceanog DEpt, La Jolla, CA 92093 USA.
[Schild, R. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Nieuwenhuizen, TM (reprint author), Inst Theoret Phys, Valckenierstr 65, NL-1018 XE Amsterdam, Netherlands.
EM t.m.nieuwenhuizen@uva.nl; cgibson@ucsd.edu; rschild@cfa.harvard.edu
RI Nieuwenhuizen, Theodorus Maria/G-8953-2012
OI Nieuwenhuizen, Theodorus Maria/0000-0002-2942-7986
NR 32
TC 7
Z9 7
U1 0
U2 1
PU EPL ASSOCIATION, EUROPEAN PHYSICAL SOCIETY
PI MULHOUSE
PA 6 RUE DES FRERES LUMIERE, MULHOUSE, 68200, FRANCE
SN 0295-5075
J9 EPL-EUROPHYS LETT
JI EPL
PD NOV
PY 2009
VL 88
IS 4
AR 49001
DI 10.1209/0295-5075/88/49001
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 533OV
UT WOS:000272835000033
ER
PT J
AU Armelagos, GJ
Goodman, AH
Harper, KN
Blakey, ML
AF Armelagos, George J.
Goodman, Alan H.
Harper, Kristin N.
Blakey, Michael L.
TI Enamel Hypoplasia and Early Mortality: Bioarcheological Support for the
Barker Hypothesis
SO EVOLUTIONARY ANTHROPOLOGY
LA English
DT Article
DE fetal programming; maternal stress; infancy; DOHaD; childhood stress;
adult mortality
ID FETAL ORIGINS HYPOTHESIS; CORONARY-HEART-DISEASE; THRIFTY PHENOTYPE
HYPOTHESIS; FOR-GESTATIONAL-AGE; HPA AXIS FUNCTION; BIRTH-WEIGHT;
BLOOD-PRESSURE; CARDIOVASCULAR-DISEASE; HERTFORDSHIRE COHORT; PRENATAL
EXPOSURE
AB The Barker hypothesis asserts that stressful events early in the life history of an individual have negative health consequences later in adulthood. The hypothesis initially focused on prenatal stressors as indicated by birth weight and related outcomes. This initial concern with the fetal phase of development led to its description as the "fetal programming" or "fetal origins" hypothesis. The realization that stressors in the postnatal phase had similar impacts on adult health has led to its latest characterization as the Developmental Origins of Health and Disease Hypothesis (DOHaD). In this paper, we review the history and evidence in support of the DOHaD hypothesis. We then introduce an untapped source of information on early life stress: enamel hypoplasias and other developmental defects of enamel. Enamel defects are nearly indelible records of physiological perturbations, or stress, to developing ameloblasts (enamel-forming cells). Furthermore, the location of the defects translates to specific periods of growth, providing a permanent temporal record of early life stressors from in utero to approximately twelve years of age. As we discuss, a handful of studies of different populations reveals that individuals with enamel defects that developed in utero and early in infant-childhood development tend to be subject to earlier adolescent or adult mortality.
C1 [Armelagos, George J.] Emory Univ, Atlanta, GA 30322 USA.
[Goodman, Alan H.] Hampshire Coll, Amherst, MA 01002 USA.
[Harper, Kristin N.] Columbia Univ, New York, NY 10027 USA.
[Blakey, Michael L.] Coll William & Mary, Inst Hist Biol, Williamsburg, VA 23187 USA.
[Blakey, Michael L.] Amer Anthropol Assoc, Prominent Museum Project, Arlington, VA USA.
[Blakey, Michael L.] Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA.
[Blakey, Michael L.] Nat Hist Museum, London, England.
[Blakey, Michael L.] New York Citys Colonial African Burial Ground Arc, New York, NY USA.
[Blakey, Michael L.] Columbia Brown Rome & Howard Univ, Spelman Coll, Washington, DC USA.
[Blakey, Michael L.] W Montague Cobb Biol Anthropol Lab, W Montague, TX USA.
RP Armelagos, GJ (reprint author), Emory Univ, Atlanta, GA 30322 USA.
EM antga@emory.edu; agoodman@hampshire.edu; kh2383@columbia.edu;
mlblak@wm.edu
RI Harper, Kristin/H-3848-2012
NR 100
TC 27
Z9 27
U1 3
U2 12
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 1060-1538
J9 EVOL ANTHROPOL
JI Evol. Anthropol.
PD NOV-DEC
PY 2009
VL 18
IS 6
BP 261
EP 271
DI 10.1002/evan.20239
PG 11
WC Anthropology
SC Anthropology
GA 540ZC
UT WOS:000273379200004
ER
PT J
AU Kidwell, PA
AF Kidwell, Peggy Aldrich
TI Computing devices, mathematics education and mathematics: Sexton's
omnimetre in its time
SO HISTORIA MATHEMATICA
LA English
DT Article
DE Sexton omnimetre; Slide rule; Numerical analysis; Albert Sexton; Joseph
Lipka
AB Material objects can tell us much about mathematical practice. In 1899, Albert Sexton, a Philadelphia mechanical engineer, received the John Scott Medal of the Franklin Institute for his invention of the omnimetre. This inexpensive circular slide rule was one of a host of computing devices that became common in the United States around 1900. It is inscribed "NUMERI MUNDUM REGUNT". In part because of instruments such as the omnimetre, numbers increasingly ruled the practical world of the late 19th and early 20th century. This changed not only engineering, but mathematics education and mathematical work. Published by Elsevier Inc.
C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA.
RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, MRC 671,POB 37012, Washington, DC 20013 USA.
EM kidwellp@si.edu
NR 27
TC 0
Z9 0
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0315-0860
J9 HIST MATH
JI Hist. Math.
PD NOV
PY 2009
VL 36
IS 4
BP 395
EP 404
DI 10.1016/j.hm.2009.06.001
PG 10
WC History & Philosophy Of Science; Mathematics, Interdisciplinary
Applications; Mathematics
SC History & Philosophy of Science; Mathematics
GA 528HU
UT WOS:000272434900004
ER
PT J
AU Horton, BM
Holberton, RL
AF Horton, Brent M.
Holberton, Rebecca L.
TI Corticosterone manipulations alter morph-specific nestling provisioning
behavior in male white-throated sparrows, Zonotrichia albicollis
SO HORMONES AND BEHAVIOR
LA English
DT Article
DE White-throated sparrow; Zonotrichia albicollis; Corticosterone; RU486;
Mifepristone; Parental care; Nestling provisioning; Self-maintenance;
Osmotic pumps
ID LONG-LIVED BIRD; AFFINITY GLUCOCORTICOID-RECEPTOR; HISTORY TRADE-OFFS;
MALE PARENTAL CARE; DARK-EYED JUNCOS; ADRENOCORTICAL-RESPONSE;
BASE-LINE; REPRODUCTIVE-PERFORMANCE; STRESS-RESPONSE; EXOGENOUS
CORTICOSTERONE
AB In the polymorphic white-throated sparrow (Zonotrichia albicollis), tan-striped males provision nestlings at higher rates than do white-striped males. In a previous study, we found that tan-striped males had lower baseline corticosterone levels than white-striped males during the nestling stage. To determine if this variation in corticosterone influences morph-specific differences in nestling provisioning behavior, we used intraperitoneal osmotic pumps to increase baseline corticosterone levels in tan-striped males (TS CORT) and administer RU486, a glucocorticoid receptor antagonist, in white-striped males (WS RU486). These manipulations essentially reversed morph-specific nestling provisioning behavior in males. TS CORT males fed nestlings at lower rates than TS controls (vehicle-only implant), and at similar rates to WS controls (vehicle-only implant), while WS RU486 males fed nestlings at higher rates than WS controls, and at similar rates to TS controls. These results demonstrate that (1) increases in baseline corticosterone (i.e., below concentrations associated with the adrenocortical response to stress) can directly or indirectly inhibit nestling provisioning behavior, and (2) corticosterone influences morph-specific variation in parental behavior in male white-throated sparrows. This study contributes to the growing evidence that modulating baseline CORT mediates parental care and self-maintenance activities in birds, and thus may serve as a mechanism for balancing current reproductive success with survival. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Horton, Brent M.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20003 USA.
[Holberton, Rebecca L.] Univ Maine, Sch Biol & Ecol, Lab Avian Biol, Orono, ME 04469 USA.
RP Horton, BM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, 3001 Connecticut Ave NW,MRC 5503, Washington, DC 20003 USA.
EM hortonb@si.edu; rebecca.holberton@maine.edu
FU Frank M. Chapman Memorial Fund; American Ornithologists' Union; Society
for Integrative and Comparative Biology; Sandpiper Technologies;
University of Maine's Association of Graduate Students; Maine
Agricultural and Forest Experiment Station; University of Maine's NSF
GK-12 [DGE-0231642]; University of Maine Graduate Research
Assistantship; Smithsonian Postdoctoral Fellowship
FX This research was funded by grants awarded to B. Horton by the Frank M.
Chapman Memorial Fund, American Ornithologists' Union, Society for
Integrative and Comparative Biology, Sandpiper Technologies, and the
University of Maine's Association of Graduate Students. Additional
research support was provided by the Maine Agricultural and Forest
Experiment Station. Graduate stipends were provided to B. Horton by the
University of Maine's NSF GK-12 Teaching Fellows Program (DGE-0231642 to
S. Brawley et al.) and a University of Maine Graduate Research
Assistantship. B. Horton was supported by a Smithsonian Postdoctoral
Fellowship during the completion of this manuscript. All field research
was conducted at the Penobscot Experimental Forest, co-managed by the
University of Maine and the U.S. Forest Service. Research assistance was
provided by M. Bougie, K. Gensel, J. Johnston, J. Kelly, J. Long, I.
Liu, and H. Murray. B. Horton would like to thank his Ph.D. advisory
committee (A. Dufty, Jr., W. Glanz, W. Halteman, and P. Marra) for their
guidance. Also, we thank T.B. Ryder and two anonymous reviewers for
their helpful comments on earlier versions of this manuscript.
NR 87
TC 18
Z9 18
U1 1
U2 14
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0018-506X
EI 1095-6867
J9 HORM BEHAV
JI Horm. Behav.
PD NOV
PY 2009
VL 56
IS 5
BP 510
EP 518
DI 10.1016/j.yhbeh.2009.09.001
PG 9
WC Behavioral Sciences; Endocrinology & Metabolism
SC Behavioral Sciences; Endocrinology & Metabolism
GA 522HG
UT WOS:000271987900004
PM 19751738
ER
PT J
AU Wang, HQ
Fisher, JA
AF Wang, Huiqun
Fisher, Jenny A.
TI North polar frontal clouds and dust storms on Mars during spring and
summer
SO ICARUS
LA English
DT Article
DE Mars
ID WATER-ICE CLOUDS; THERMAL EMISSION SPECTROMETER; ORBITER CAMERA
OBSERVATIONS; GENERAL-CIRCULATION MODEL; TES NADIR DATA; MARTIAN
ATMOSPHERE; INTERANNUAL VARIABILITY; GLOBAL-SURVEYOR; MGS TES; MAPPING
YEAR
AB The complete archive of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) Mars Daily Global Maps (MDGM) are used to Study north polar clouds and dust storms that exhibit frontal structures during the spring and summer (L-s 0-180 degrees). Results show that frontal events generally follow the edge of the polar cap during spring and mid/late summer with a gap in the distribution in early Summer. The exact duration and timing of the gal vary from year to year. Ten to twenty percent of spring and summer time frontal events exhibit complex morphologies. Distinct temperature signatures are associated with features observed in images in many but not all cases. The general travel paths of the frontal events are eastward around the polar cap. Westward paths exist only at the edge of the polar cap in late spring/early summer. Occasionally, the paths curve toward or away from the polar cap in certain longitude sectors. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Wang, Huiqun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fisher, Jenny A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
RP Wang, HQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hwang@cfa.harvard.edu
RI Fisher, Jenny/J-3979-2012
OI Fisher, Jenny/0000-0002-2921-1691
FU NASA Mars Data Analysis
FX This study is supported by NASA Mars Data Analysis program. We thank
Daniel Tyler Jr. for providing comments on improving our manuscript. We
thank R. John Wilson and Mark I. Richardson for their thoughtful
reviews.
NR 49
TC 8
Z9 8
U1 0
U2 7
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 NOV
PY 2009
VL 204
IS 1
BP 103
EP 113
DI 10.1016/j.icarus.2009.05.028
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 507VT
UT WOS:000270884100008
ER
PT J
AU Yamanoue, Y
Johnson, GD
Starnes, WC
AF Yamanoue, Yusuke
Johnson, G. David
Starnes, Wayne C.
TI Redescription of a poorly known acropomatid, Verilus sordidus Poey 1860,
and comparison with Neoscombrops atlanticus Mochizuki and Sano 1984
(Teleostei: Perciformes)
SO ICHTHYOLOGICAL RESEARCH
LA English
DT Article
DE Verilus sordidus; Neoscombrops atlanticus; Acropomatidae; Anal-fin
pterygiophore
ID PERCICHTHYID FISH; GENUS; ANNECTENS; PACIFICUS; SYNONYM; JAPAN
AB A poorly known acropomatid, Verilus sordidus Poey 1860, is redescribed based on six specimens from the western central Atlantic. We present diagnostic characters to differentiate this species from Neoscombrops atlanticus Mochizuki and Sano 1984, which has been confused with this species, and designate a neotype of V. sordidus. This species is distinguishable from N. atlanticus by the proximal-middle radial of the first anal-fin pterygiophore being slender with no trough or hollow on the anterodorsal portion (vs. hollow in N. atlanticus), several canine teeth posterior to the large canine teeth on either side of the symphysis of the lower jaw (vs. villiform teeth posterior to enlarged canines), and by the modal numbers of pectoral-fin rays, lateral-line scales, and gill rakers on the lower limb of the first arch.
C1 [Yamanoue, Yusuke] Univ Tokyo, Ocean Res Inst, Nakano Ku, Tokyo 1648639, Japan.
[Johnson, G. David] Smithsonian Inst, MRC 159, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA.
[Starnes, Wayne C.] N Carolina Museum Nat Sci, Res Lab, Raleigh, NC 27699 USA.
RP Yamanoue, Y (reprint author), Univ Tokyo, Ocean Res Inst, Nakano Ku, 1-15-1 Minamidai, Tokyo 1648639, Japan.
EM yamanouey@yahoo.co.jp
FU Ito Grant for Ichthyology; Fujiwara Natural History Foundation; Japan
Society for the Promotion of Science for Young Scientists [10824]
FX We are grateful to the following persons and institutions for specimen
loans: D. Catania (CAS), K. Hartel (MCZ), S. Jewett, L. Palmer, S.
Raredon, J. Williams, and R. Vari (USNM). W. Eschmeyer (CAS), K. Hartel
(MCZ), and B. Collette (Systematics Laboratory, NMFS) kindly provided us
with helpful comments on type specimens of Verilus sordidus. The first
author also thanks A. Charef (Univ. Tokyo), who kindly translated the
French description of Poey (1860), and A. Carvalho-Filho (Fish Bizz
Ltda) for helpful comments. A portion of this study was supported by the
Ito Grant for Ichthyology, Fujiwara Natural History Foundation, and
Research Fellowship of the Japan Society for the Promotion of Science
for Young Scientists (10824).
NR 29
TC 2
Z9 2
U1 0
U2 0
PU SPRINGER TOKYO
PI TOKYO
PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN
SN 1341-8998
J9 ICHTHYOL RES
JI Ichthyol. Res.
PD NOV
PY 2009
VL 56
IS 4
BP 400
EP 406
DI 10.1007/s10228-009-0131-0
PG 7
WC Zoology
SC Zoology
GA 516LC
UT WOS:000271542700011
ER
PT J
AU Bradley, TJ
Briscoe, AD
Brady, SG
Contreras, HL
Danforth, BN
Dudley, R
Grimaldi, D
Harrison, JF
Kaiser, JA
Merlin, C
Reppert, SM
VandenBrooks, JM
Yanoviak, SR
AF Bradley, Timothy J.
Briscoe, Adriana D.
Brady, Sean G.
Contreras, Heidy L.
Danforth, Bryan N.
Dudley, Robert
Grimaldi, David
Harrison, Jon F.
Kaiser, J. Alexander
Merlin, Christine
Reppert, Steven M.
VandenBrooks, John M.
Yanoviak, Steve R.
TI Episodes in insect evolution
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article; Proceedings Paper
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
CY JAN 03-07, 2011
CL Salt Lake City, UT
SP Soc Integrat & Comparat Biol
ID HALICTUS-RUBICUNDUS HYMENOPTERA; DIRECTED AERIAL DESCENT; ALLODAPINE
BEES; SOCIAL EVOLUTION; MOLECULAR PHYLOGENETICS; GENE DUPLICATION;
CIRCADIAN CLOCK; NESTING BIOLOGY; MARINE HEXAPOD; MESSENGER-RNAS
AB This article derives from a society-wide symposium organized by Timothy Bradley and Adriana Briscoe and presented at the 2009 annual meeting of the Society for Integrative and Comparative Biology in Boston, Massachusetts. David Grimaldi provided the opening presentation in which lie outlined the major evolutionary events in the formation and subsequent diversification of the insect clade. This presentation was followed by speakers who detailed the evolutionary history of specific physiological and/or behavioral traits that have caused insects to be both ecologically successful and fascinating as subjects for biological study. These include a review of the evolutionary history of the insects, the origins of flight, osmoregulation, the evolution of tracheal systems, the evolution of color vision, circadian clocks, and the evolution of eusociality. These topics, as covered by the speakers, provide an overview of the pattern and timing of evolutionary diversification and specialization in the group of animals we know as insects.
C1 [Bradley, Timothy J.; Briscoe, Adriana D.; Contreras, Heidy L.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
[Brady, Sean G.] Smithsonian Inst, Natl Museum, Dept Entomol, Washington, DC 20013 USA.
[Brady, Sean G.] Smithsonian Inst, Natl Museum, Labs Analyt Biol, Washington, DC 20013 USA.
[Danforth, Bryan N.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA.
[Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Grimaldi, David] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA.
[Harrison, Jon F.; VandenBrooks, John M.] Arizona State Univ, Sch Life Sci, Sect Organismal Integrat & Syst Biol, Tempe, AZ 85287 USA.
[Kaiser, J. Alexander] Midwestern Univ, Dept Basic Sci, Glendale, AZ 85308 USA.
[Merlin, Christine; Reppert, Steven M.] Univ Massachusetts, Sch Med, Dept Neurobiol, Worcester, MA 01605 USA.
[Yanoviak, Steve R.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
RP Bradley, TJ (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
EM tbradley@uci.edy
RI Briscoe, Adriana/E-8963-2010
OI Briscoe, Adriana/0000-0001-8514-4983
NR 149
TC 27
Z9 27
U1 5
U2 46
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD NOV
PY 2009
VL 49
IS 5
BP 590
EP 606
DI 10.1093/icb/icp043
PG 17
WC Zoology
SC Zoology
GA 521TH
UT WOS:000271946500010
PM 21665843
ER
PT J
AU Ortner, DJ
AF Ortner, D. J.
TI HUMAN REMAINS IN ARCHAEOLOGY: A HANDBOOK
SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY
LA English
DT Book Review
C1 [Ortner, D. J.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA.
RP Ortner, DJ (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 3
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 1047-482X
J9 INT J OSTEOARCHAEOL
JI Int. J. Osteoarchaeol.
PD NOV-DEC
PY 2009
VL 19
IS 6
BP 751
EP 752
DI 10.1002/oa.1115
PG 2
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 532DJ
UT WOS:000272724600009
ER
PT J
AU Ross, AH
Ubelaker, DH
AF Ross, Ann H.
Ubelaker, Douglas H.
TI Effect of Intentional Cranial Modification on Craniofacial Landmarks: A
Three-Dimensional Perspective
SO JOURNAL OF CRANIOFACIAL SURGERY
LA English
DT Article
DE Craniofacial morphology; deformed crania; geometric morphometrics
ID VAULT MODIFICATION; DEFORMATION; BASE; FACE
AB Although processes of cranial modification have been documented throughout the world, the effects on craniofacial landmarks are poorly understood. Such understanding is needed to assist the further understanding of craniofacial morphology and dysmorphology and in the interpretation of craniometric studies assessing issues of biological distance. Samples of both clinically normal and modified crania recovered from the same archeological site in Peru were studied using a three-dimensional approach to evaluate differences in landmark location. The crania were associated with the Ancon site from the central coast, corresponding to the Late Intermediate period (AD 900-1300). Analysis revealed that vault modification had no significant effect on the locations of landmarks of the facial and basal regions. As expected, differences were found on some landmarks of the cranial vault.
C1 [Ross, Ann H.] N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA.
[Ubelaker, Douglas H.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Ross, AH (reprint author), N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA.
EM ann_rose@ncsu.edu
OI Ross, Ann/0000-0001-8780-1414
NR 22
TC 9
Z9 9
U1 0
U2 6
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 1049-2275
J9 J CRANIOFAC SURG
JI J. Craniofac. Surg.
PD NOV
PY 2009
VL 20
IS 6
BP 2185
EP 2187
DI 10.1097/SCS.0b013e3181bf038c
PG 3
WC Surgery
SC Surgery
GA 526SL
UT WOS:000272313600049
PM 19934673
ER
PT J
AU Ruger, N
Huth, A
Hubbell, SP
Condit, R
AF Rueger, Nadja
Huth, Andreas
Hubbell, Stephen P.
Condit, Richard
TI Response of recruitment to light availability across a tropical lowland
rain forest community
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE Barro Colorado Island; hierarchical Bayesian model; life-history traits;
light requirements; niche partitioning; Panama; regeneration niche;
shade tolerance; tropical rain forest
ID NEOTROPICAL FOREST; TREE DIVERSITY; CANOPY GAPS; DIPTEROCARP SEEDLINGS;
SPECIES-DIVERSITY; MOIST FOREST; COSTA-RICA; NICHE; DISTRIBUTIONS;
REGENERATION
AB P> Many hypotheses about species coexistence involve differential resource use and trade-offs in species' life-history traits. Quantifying resource use across most species in diverse communities, although, has seldom been attempted.
We use a hierarchical Bayesian approach to quantify the light dependence of recruitment in 263 woody species in a 50-ha long-term forest census plot in Panama. Data on sapling recruitment were obtained using the 1985-1990 and 1990-1995 census intervals. Available light was estimated for each recruit from yearly censuses of canopy density.
We use a power function (linear log-log relationship) to model the light effect on recruitment. Different responses of recruitment to light are expressed by the light effect parameter b. The distribution of b had a central mode at 0.8, suggesting that recruitment of many species responds nearly linearly to increasing light.
Nearly every species showed increases in recruitment with increasing light. Just nine species (3%) had recruitment declining with light, while 198 species (75%) showed increasing recruitment in both census intervals. Most of the increases in recruitment were decelerating, i.e. the increase was less at higher light (b < 1). In the remaining species, the response to light varied between census intervals (24 species) or species did not have recruits in both intervals (41 species).
Synthesis. Nearly all species regenerate better in higher light, and recruitment responses to light are spread along a continuum ranging from modest increase with light to a rather strict requirement for high light. These results support the hypothesis that spatio-temporal variation in light availability may contribute to the diversity of tropical tree species by providing opportunities for niche differentiation with respect to light requirements for regeneration.
C1 [Rueger, Nadja; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Condit, Richard] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA.
[Condit, Richard] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA.
RP Ruger, N (reprint author), Tech Univ Dresden, Dept Forest Biometr Syst Anal, Inst Forest Growth & Forest Comp Sci, Pienner Str 8, D-01737 Tharandt, Germany.
EM nadja.rueger@tu-dresden.de
RI Ruger, Nadja/J-6393-2015
OI Ruger, Nadja/0000-0003-2371-4172
FU Center for Tropical Forest Science; National Center for Ecological
Analysis and Synthesis (Santa Barbara, CA, USA); U.S. National Science
Foundation; John D. and Catherine D. McArthur Foundation; Smithsonian
Tropical Research Institute
FX We thank Liza Comita and Ines Ibanez for advice on hierarchical Bayesian
modelling, Helene Muller-Landau for providing the step width-adjusting
routine of the Metropolis-Hastings algorithm, and Helene Muller-Landau
and Robin Chazdon for valuable comments on the manuscript. N.R. was
supported by a research grant from the Center for Tropical Forest
Science, and R.C. by a fellowship from the National Center for
Ecological Analysis and Synthesis (Santa Barbara, CA, USA). The BCI plot
has been made possible through the support of the U.S. National Science
Foundation, the John D. and Catherine D. McArthur Foundation and the
Smithsonian Tropical Research Institute. We thank the dozens of field
assistants and botanists who have collected data on trees and carried
out the canopy censuses in the BCI plot over the past 25 years.
NR 58
TC 37
Z9 38
U1 6
U2 47
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD NOV
PY 2009
VL 97
IS 6
BP 1360
EP 1368
DI 10.1111/j.1365-2745.2009.01552.x
PG 9
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 506PH
UT WOS:000270787100026
ER
PT J
AU Bachvaroff, TR
Place, AR
Coats, DW
AF Bachvaroff, Tsvetan R.
Place, Allen R.
Coats, Donald Wayne
TI Expressed Sequence Tags from Amoebophrya sp Infecting Karlodinium
veneficum: Comparing Host and Parasite Sequences
SO JOURNAL OF EUKARYOTIC MICROBIOLOGY
LA English
DT Article
DE Expressed genes; parasitism; Syndiniales; transcriptome
ID PHYLOGENETIC POSITION; GENETIC DIVERSITY; KARENIA-BREVIS;
DINOFLAGELLATE; STRAINS; CULTURE; GENOME; PROTISTS; GROWTH; CYCLE
AB Parasitic dinoflagellates of the genus Amoebophrya play important roles in the ecology of estuaries and open ocean environments. Little is known of the cell and molecular biology of Amoebophrya, but the genus is intermediate on phylogenetic trees between apicomplexans and typical dinophycean dinoflagellates. Here, we constructed four cDNA libraries, from different stages after infecting the host, Karlodinium veneficum, with Amoebophrya sp. These libraries were used to generate 898 expressed sequence tags (ESTs), with sequences attributed to either the host or parasite, based on AT bias, codon usage, and occurrence during infection. Overall, 209 sequences were attributable to the parasite and 685 to the host. The 50 putative parasite sequences with good protein matches in GenBank were used to find the same protein from host ESTs. For 26 genes, both host and parasite sequences were identified, of which 20 encoded ribosomal proteins. PCR for seven predicted parasite and two host genes were used to confirm attributions. The most common host and parasite ESTs were compared to see if multiple gene copies were present. The host plastocyanin gene had multiple sequence variants, but parasite rps27a contained only one polymorphism, likely due to an amplification error. Amplification, cloning, and sequencing of five parasite protein-coding genes suggested that the parasite has a single sequence for each gene, but three host genes were found to have multiple variants. The genome of Amoebophrya sp. infecting K. veneficum appears to have an organization more similar to other eukaryotes than to the tandem gene arrangements found in dinoflagellates.
C1 [Bachvaroff, Tsvetan R.; Coats, Donald Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Place, Allen R.] Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, Baltimore, MD 21202 USA.
RP Bachvaroff, TR (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM bachvarofft@si.edu
RI Place, Allen/F-9267-2013
FU NOAA [NA04NOS4780276]; University of Maryland Biotechnology Institute;
NSF [EF-0629624]; Center of Marine Biotechnology [09-205]; ECOHAB
program [310]
FX The authors would like to thank Matthew Fienberg, Holly Bowers, Ernest
Williams, and Sara Handy for assistance. Grant support was provided by
NOAA Coastal Ocean Program award NA04NOS4780276 to A. R. Place and the
University of Maryland Biotechnology Institute and NSF ATOL Award
EF-0629624. This is contribution 09-205 from the Center of Marine
Biotechnology and contribution 310 from the ECOHAB program.
NR 45
TC 13
Z9 13
U1 1
U2 8
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1066-5234
J9 J EUKARYOT MICROBIOL
JI J. Eukaryot. Microbiol.
PD NOV-DEC
PY 2009
VL 56
IS 6
BP 531
EP 541
DI 10.1111/j.1550-7408.2009.00433.x
PG 11
WC Microbiology
SC Microbiology
GA 511SV
UT WOS:000271188700004
PM 19883441
ER
PT J
AU Cardona, A
Valencia, V
Bayona, G
Jaramillo, C
Ojeda, G
Ruiz, J
AF Cardona, A.
Valencia, V.
Bayona, G.
Jaramillo, C.
Ojeda, G.
Ruiz, J.
TI U/Pb LA-MC-ICP-MS Zircon Geochronology and Geochemistry from a
Postcollisional Biotite Granite of the Baja Guajira Basin, Colombia:
Implications for Late Cretaceous and Neogene Caribbean-South American
Tectonics
SO JOURNAL OF GEOLOGY
LA English
DT Article
ID SIERRA-DE-PERIJA; CENOZOIC SEDIMENTATION; CONTINENTAL-CRUST; SLAB
DETACHMENT; VOLCANIC-ROCKS; EASTERN CUBA; MAGMATISM; EVOLUTION; ARC;
VENEZUELA
AB U/Pb LA-MC-ICP-MS zircon ages and whole-rock geochemistry from a biotite granitoid, recovered at similar to 2.1 km depth from the Rancheria-2 well in the Baja Guajira basin, southern Caribbean region, reveal the existence of a ca. 70 Ma silicic plutonic event. This granitoid intrudes ca. 76-80 Ma intraoceanic arc fragments and continental margin sediments that experienced continental subduction and collision since ca. 76 Ma. The major compositional shift recorded by this granitoid, including light rare earth element (LREE) enrichment ([La/Yb](N) = 11.28), the increase in the arc maturity and its postcollisional affinity, suggests that this magmatism may have been formed during the waning stages of collision due to slab break-off that followed the end of the continental subduction. This interpretation would constrain arc-continent collision of the allochthonous Caribbean plate with this segment of the continental margin by ca. 70-76 Ma. Contemporaneous and slightly diachronous accretionary events are seen along most of the northwestern South American margin. We therefore suggest that the oblique geometry of the Caribbean-South American plate interactions facilitates the accretion of the eastern and northern segments of the oceanic plate margins. Unconformable contact with Late Oligocene-Early Miocene sediments suggests that the granitoid and its host rocks were uplifted and exhumed between the Late Maastrichtian and the Late Oligocene as a consequence of the major changes on the Caribbean-South American convergence.
C1 Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
Ecopetrol, Inst Colombiano Petroleo, Piedecuesta 4185, Santander, Colombia.
RP Cardona, A (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
EM cardonaa@si.edu
FU Ecopetrol-ICP; Banco de la Repu publica de Colombia [2289]; Arizona
LaserChron Center [EAR-0443387]; National Science Foundation
FX Support from Ecopetrol-ICP is highly appreciated. The staff of the
Litoteca Nacional of the Agencia Nacional de Hidrocarburos is
acknowledged for their help during sampling. Discussions and support
from M. Weber, O. Mantilla, and V. Torres are also greatly appreciated.
Thorough and clear reviews and suggestions by J. Pindell and an
anonymous reviewer and the editorial care of D. Rowley are gratefully
acknowledged. This research has received support from a grant of the
Banco de la Repu publica de Colombia, project 2289. Funding for the
Arizona LaserChron Center is provided partially by grant EAR-0443387
from the National Science Foundation. This is a contribution to project
IGCP-546, "Subduction Zones of the Caribbean."
NR 59
TC 11
Z9 11
U1 1
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0022-1376
J9 J GEOL
JI J. Geol.
PD NOV
PY 2009
VL 117
IS 6
BP 685
EP 692
DI 10.1086/605776
PG 8
WC Geology
SC Geology
GA 501HR
UT WOS:000270372700007
ER
PT J
AU Haussler, D
O'Brien, SJ
Ryder, OA
Barker, FK
Clamp, M
Crawford, AJ
Hanner, R
Hanotte, O
Johnson, WE
McGuire, JA
Miller, W
Murphy, RW
Murphy, WJ
Sheldon, FH
Sinervo, B
Venkatesh, B
Wiley, EO
Allendorf, FW
Amato, G
Baker, CS
Bauer, A
Beja-Pereira, A
Bermingham, E
Bernardi, G
Bonvicino, CR
Brenner, S
Burke, T
Cracraft, J
Diekhans, M
Edwards, S
Ericson, PGP
Estes, J
Fjelsda, J
Flesness, N
Gamble, T
Gaubert, P
Graphodatsky, AS
Graves, JAM
Green, ED
Green, RE
Hackett, S
Hebert, P
Helgen, KM
Joseph, L
Kessing, B
Kingsley, DM
Lewin, HA
Luikart, G
Martelli, P
Moreira, MAM
Nguyen, N
Orti, G
Pike, BL
Rawson, DM
Schuster, SC
Seuanez, HN
Shaffer, HB
Springer, MS
Stuart, JM
Sumner, J
Teeling, E
Vrijenhoek, RC
Ward, RD
Warren, WC
Wayne, R
Williams, TM
Wolfe, ND
Zhang, YP
Graph-Odatsky, A
Johnson, WE
Felsenfeld, A
Turner, S
AF Haussler, David
O'Brien, Stephen J.
Ryder, Oliver A.
Barker, F. Keith
Clamp, Michele
Crawford, Andrew J.
Hanner, Robert
Hanotte, Olivier
Johnson, Warren E.
McGuire, Jimmy A.
Miller, Webb
Murphy, Robert W.
Murphy, William J.
Sheldon, Frederick H.
Sinervo, Barry
Venkatesh, Byrappa
Wiley, Edward O.
Allendorf, Fred W.
Amato, George
Baker, C. Scott
Bauer, Aaron
Beja-Pereira, Albano
Bermingham, Eldredge
Bernardi, Giacomo
Bonvicino, Cibele R.
Brenner, Sydney
Burke, Terry
Cracraft, Joel
Diekhans, Mark
Edwards, Scott
Ericson, Per G. P.
Estes, James
Fjelsda, Jon
Flesness, Nate
Gamble, Tony
Gaubert, Philippe
Graphodatsky, Alexander S.
Graves, Jennifer A. Marshall
Green, Eric D.
Green, Richard E.
Hackett, Shannon
Hebert, Paul
Helgen, Kristofer M.
Joseph, Leo
Kessing, Bailey
Kingsley, David M.
Lewin, Harris A.
Luikart, Gordon
Martelli, Paolo
Moreira, Miguel A. M.
Nguyen, Ngan
Orti, Guillermo
Pike, Brian L.
Rawson, David Michael
Schuster, Stephan C.
Seuanez, Hector N.
Shaffer, H. Bradley
Springer, Mark S.
Stuart, Joshua Michael
Sumner, Joanna
Teeling, Emma
Vrijenhoek, Robert C.
Ward, Robert D.
Warren, Wesley C.
Wayne, Robert
Williams, Terrie M.
Wolfe, Nathan D.
Zhang, Ya-Ping
Graph-Odatsky, Alexander
Johnson, Warren E.
Felsenfeld, Adam
Turner, Steve
CA Genome 10K Community Scientists
Mammals Grp
Birds Grp
Amphibians Reptiles Grp
Fishes Grp
General Policy Grp
Anal Grp
TI Genome 10K: A Proposal to Obtain Whole-Genome Sequence for 10 000
Vertebrate Species
SO JOURNAL OF HEREDITY
LA English
DT Article
DE ancestral state reconstruction; comparative genomics; G10K; molecular
evolution; species conservation; vertebrate biology
ID PLURIPOTENT STEM-CELLS; ANTIMICROBIAL PEPTIDES; MOLECULAR PHYLOGENY;
DIVERGENCE TIMES; POISON FROGS; EVOLUTION; GENERATION; CONSERVATION;
GENETICS; ORIGINS
AB The human genome project has been recently complemented by whole-genome assessment sequence of 32 mammals and 24 nonmammalian vertebrate species suitable for comparative genomic analyses. Here we anticipate a precipitous drop in costs and increase in sequencing efficiency, with concomitant development of improved annotation technology and, therefore, propose to create a collection of tissue and DNA specimens for 10 000 vertebrate species specifically designated for whole-genome sequencing in the very near future. For this purpose, we, the Genome 10K Community of Scientists (G10KCOS), will assemble and allocate a biospecimen collection of some 16 203 representative vertebrate species spanning evolutionary diversity across living mammals, birds, nonavian reptiles, amphibians, and fishes (ca. 60 000 living species). In this proposal, we present precise counts for these 16 203 individual species with specimens presently tagged and stipulated for DNA sequencing by the G10KCOS. DNA sequencing has ushered in a new era of investigation in the biological sciences, allowing us to embark for the first time on a truly comprehensive study of vertebrate evolution, the results of which will touch nearly every aspect of vertebrate biological enquiry.
C1 [Haussler, David] Univ Calif Santa Cruz, Howard Hughes Med Inst, Santa Cruz, CA 95064 USA.
[O'Brien, Stephen J.; Johnson, Warren E.] NCI, Lab Genom Divers, Frederick, MD 21701 USA.
[Ryder, Oliver A.] San Diego Zoos Inst Conservat Res, Escondido, CA USA.
[Barker, F. Keith] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
[Clamp, Michele] Broad Inst MIT & Harvard, Cambridge, MA USA.
[Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia.
[Hanner, Robert] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
[Hanotte, Olivier] Univ Nottingham, Sch Biol, Frozen Ark Project, Nottingham, Northants, England.
[McGuire, Jimmy A.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
[McGuire, Jimmy A.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Miller, Webb] Penn State Univ, Dept Biol, University Pk, PA 16802 USA.
[Murphy, Robert W.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada.
[Murphy, William J.] Texas A&M Univ, Dept Vet Integrat Biosci, College Stn, TX USA.
[Sheldon, Frederick H.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Sheldon, Frederick H.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Williams, Terrie M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Ctr Ocean Hlth, Santa Cruz, CA 95064 USA.
[Venkatesh, Byrappa] Agcy Sci Technol & Res, Inst Mol & Cell Biol, Singapore, Singapore.
[Wiley, Edward O.] Univ Kansas, Museum Nat Hist, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
[Wiley, Edward O.] Univ Kansas, Biodivers Res Ctr, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
[Allendorf, Fred W.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA.
[Amato, George] Amer Museum Nat Hist, Ctr Conservat Genet, New York, NY 10024 USA.
[Baker, C. Scott] Oregon State Univ, Marine Mammal Inst, Newport, OR USA.
[Baker, C. Scott] Oregon State Univ, Dept Fisheries & Wildlife, Newport, OR USA.
[Bauer, Aaron] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
[Beja-Pereira, Albano] CIBIO, Maonte Crasto, Vairao, Portugal.
[Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Seuanez, Hector N.] Univ Fed Rio de Janeiro, Inst Nacl Canc, Div Genet, BR-20231050 Rio De Janeiro, Brazil.
[Bonvicino, Cibele R.] Fundacao Oswaldo Cruz, Inst Oswaldo Cruz, Lab Biol & Parasitol Mamiferos Reservatorios Silv, Rio De Janeiro, Brazil.
[Brenner, Sydney] Salk Inst Biol Studies, San Diego, CA USA.
[Brenner, Sydney] Okinawa Inst Sci & Technol, Okinawa, Japan.
[Burke, Terry] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA.
[Edwards, Scott] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Ericson, Per G. P.] Swedish Museum Nat Hist, S-10405 Stockholm, Sweden.
[Estes, James] Ctr Ocean Hlth, Dept Ecol & Evolut, Santa Cruz, CA USA.
[Fjelsda, Jon] Univ Copenhagen, Zool Museum, DK-1168 Copenhagen, Denmark.
[Flesness, Nate] ISIS, Minneapolis, MN USA.
[Gamble, Tony] Univ Minnesota, Dept Genet & Cell Biol, Minneapolis, MN 55455 USA.
[Gaubert, Philippe] Museum Natl Hist Nat, UMR BOREA IRD 207, F-75231 Paris, France.
[Graphodatsky, Alexander S.] Russian Acad Sci, Siberian Branch, Inst Chem Biol & Fundamental Med, Novosibirsk, Russia.
[Graves, Jennifer A. Marshall] Australian Natl Univ, Res Sch Biol, Canberra, ACT, Australia.
[Green, Eric D.] NHGRI, NIH, Bethesda, MD 20892 USA.
[Green, Richard E.] Max Planck Inst Evolutionary Anthropol, Leipzig, Germany.
[Hackett, Shannon] Field Museum Nat Hist, Dept Zool, Div Birds, Chicago, IL 60605 USA.
[Hebert, Paul] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
[Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA.
[Joseph, Leo] CSIRO Sustainable Ecosyst Gungahlin Homestead, Canberra, ACT, Australia.
[Kessing, Bailey] NCI, SAIC Frederick Inc, Lab Genom Div, Frederick, MD 21701 USA.
[Kingsley, David M.] HHMI, Stanford, CA USA.
[Kingsley, David M.] Stanford Univ, Beckman Ctr, Stanford, CA USA.
[Lewin, Harris A.] Univ Illinois, Dept Anim Sci, Urbana, IL 61801 USA.
[Lewin, Harris A.] Univ Illinois, Inst Genom Biol, Urbana, IL 61801 USA.
[Luikart, Gordon] Univ Porto, Ctr Investigacao Biodiversidade & Recursos Genet, Univ Montana, Div Biol Sci,CIBIO, Missoula, MT 59812 USA.
[Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.
[Pike, Brian L.; Wolfe, Nathan D.] Global Viral Forecasting Initiat, San Francisco, CA USA.
[Rawson, David Michael] Univ Bedfordshire, LIRANS Inst, Luton, Beds, England.
[Seuanez, Hector N.] Univ Fed Rio de Janeiro, Dept Genet, BR-21949570 Rio De Janeiro, Brazil.
[Shaffer, H. Bradley] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA.
[Shaffer, H. Bradley] Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA.
[Springer, Mark S.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA.
[Sumner, Joanna] Museum Victoria, Melbourne, Vic, Australia.
[Teeling, Emma] Univ Coll Dublin, Sch Biol & Environm Sci, Sci Ctr W, Dublin 2, Ireland.
[Vrijenhoek, Robert C.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA.
[Ward, Robert D.] CSIRO Marine & Atmospher Res, Hobart, Tas, Australia.
[Warren, Wesley C.] Washington Univ, Sch Med, Genome Sequencing Ctr, St Louis, MO USA.
[Wayne, Robert] Univ Calif Los Angeles, Los Angeles, CA USA.
[Wolfe, Nathan D.] Stanford Univ, Program Human Biol, Stanford, CA 94305 USA.
[Zhang, Ya-Ping] Chinese Acad Sci, Kunming Inst Zool, State Key Lab Genet Resources & Evolut, Kunming, Yunnan, Peoples R China.
RP Haussler, D (reprint author), Univ Calif Santa Cruz, Howard Hughes Med Inst, CBSE ITI E2501, Santa Cruz, CA 95064 USA.
EM haussler@soe.ucsc.edu; stephen.obrien@nih.gov; oryder@sandiegozoo.org
RI Johnson, Warren/D-4149-2016; Beja-Pereira, Albano/B-3681-2008; Joseph,
Leo/F-9235-2010; Murphy, Robert/D-8586-2011; Bernardi,
Giacomo/F-6346-2011; Gamble, Tony/A-5690-2011; Ward, Robert/A-2319-2012;
ASTAR, IMCB/E-2320-2012; Barker, Keith/K-2795-2012; Hanotte,
Olivier/B-4669-2013; Bonvicino, Cibele /O-3390-2014; Graphodatsky,
Alexander/B-4922-2010; Inca, Inct/K-2204-2013; Burke, Terry/B-3196-2011
OI Johnson, Warren/0000-0002-5954-186X; Luikart,
Gordon/0000-0001-8697-0582; Rawson, David/0000-0002-0289-3856; Edwards,
Scott/0000-0003-2535-6217; Venkatesh, Byrappa/0000-0003-3620-0277;
Beja-Pereira, Albano/0000-0002-1607-7382; Bernardi,
Giacomo/0000-0002-8249-4678; Barker, Keith/0000-0001-7488-2470;
Graphodatsky, Alexander/0000-0002-8282-1085; Burke,
Terry/0000-0003-3848-1244
FU American Genetic Association,; Gordon and Betty Moore Foundation; NHGRI
Intramural Sequencing Center; UCSC Alumni Association; Howard Hughes
Medical Institute; Euteleost Tree of Life; National Science Foundation
[0732819, DEB-0640967, 0543556, 0817042, EF0629849, DEB-0443470,
30621092]; The Global Viral Forecasting Initiative; Biomedical Research
Council of A*STAR, Singapore; Natural Sciences and Engineering Research
Council Discovery Grant; National Basic Research Program of China
[2007CB411600]; Bureau of Science and Technology of Yunnan Province;
MCB; SB RAS Programs; Portuguese-American Foundation for Development,
CIBIO, UP, University of Montana; Portuguese Science Foundation
[PTDC/CVT/69438/2006, PTDC/BIA-BDE/65625/2006]
FX American Genetic Association, Gordon and Betty Moore Foundation, NHGRI
Intramural Sequencing Center, and UCSC Alumni Association to cost of the
Genome 10K workshop; Howard Hughes Medical Institute to D. H.; Gordon
and Betty Moore Foundation to S. C. S.; Assembling the Euteleost Tree of
Life to E. W.; National Science Foundation (0732819 to E. W.,
DEB-0640967 and 0543556 to J. A. M., 0817042 to H. B. S., EF0629849 to
W. J. M., DEB-0443470 to G. O.); The Global Viral Forecasting Initiative
to N. W., B. P., and M. L.; Biomedical Research Council of A*STAR,
Singapore to B. V.; Natural Sciences and Engineering Research Council
Discovery Grant to R. W. M.; National Basic Research Program of China
(973 Program, 2007CB411600), the National Natural Science Foundation of
China (30621092), and Bureau of Science and Technology of Yunnan
Province to Y. Z.; MCB and SB RAS Programs (A. S. G.);
Portuguese-American Foundation for Development, CIBIO, UP, University of
Montana [G. L.] and Portuguese Science Foundation [PTDC/CVT/69438/2006;
PTDC/BIA-BDE/65625/2006 to G. L].
NR 94
TC 204
Z9 208
U1 4
U2 61
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-1503
EI 1465-7333
J9 J HERED
JI J. Hered.
PD NOV-DEC
PY 2009
VL 100
IS 6
BP 659
EP 674
DI 10.1093/jhered/esp086
PG 16
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 520CN
UT WOS:000271817600001
ER
PT J
AU Larson, SG
Jungers, WL
Tocheri, MW
Orr, CM
Morwood, MJ
Sutikna, T
Awe, RD
Djubiantono, T
AF Larson, S. G.
Jungers, W. L.
Tocheri, M. W.
Orr, C. M.
Morwood, M. J.
Sutikna, T.
Awe, Rokhus Due
Djubiantono, T.
TI Descriptions of the upper limb skeleton of Homo floresiensis
SO JOURNAL OF HUMAN EVOLUTION
LA English
DT Article
DE Homo floresiensis; scapula; clavicle; humerus; radius; ulna; carpals;
phalanges
ID LATE PLEISTOCENE; HOMININ; INDONESIA; AUSTRALOPITHECUS; MORPHOLOGY;
EVOLUTION; SHOULDER; PRIMATES; SAPIENS; HUMERI
AB Several bones of the upper extremity were recovered during excavations of Late Pleistocene deposits at Liang Bua, Flores, and these have been attributed to Homo floresiensis. At present, these upper limb remains have been assigned to six different individuals - LB1, LB2, LB3, LB4, LB5, and LB6. Several of these bones are complete or nearly so, but some are quite fragmentary. All skeletal remains recovered from Liang Bua were extremely fragile, but have now been stabilized and hardened in the laboratory in Jakarta. They are now curated in museum-quality containers at the National Research and Development Centre for Archaeology in Jakarta, Indonesia. These skeletal remains are described and illustrated photographically. The upper limb presents a unique mosaic of derived (human-like) and primitive morphologies, the combination of which is never found in either healthy or pathological modem humans. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Larson, S. G.; Jungers, W. L.] SUNY Stony Brook, Dept Anat Sci, Med Ctr, Sch Med, Stony Brook, NY 11794 USA.
[Tocheri, M. W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA.
[Orr, C. M.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA.
[Orr, C. M.] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA.
[Morwood, M. J.] Univ Wollongong, Sch Earth & Environm Sci, GeoQuEST Res Ctr, Wollongong, NSW 2522, Australia.
[Sutikna, T.; Awe, Rokhus Due] Indonesian Ctr Archaeol, Jakarta 12001, Indonesia.
[Morwood, M. J.] Univ New England, Sch Human & Environm Studies, Armidale, NSW 2351, Australia.
[Djubiantono, T.] Natl Res & Dev Ctr Archaeol, Jakarta, Indonesia.
RP Larson, SG (reprint author), SUNY Stony Brook, Dept Anat Sci, Med Ctr, Sch Med, Stony Brook, NY 11794 USA.
EM susan.larson@stonybrook.edu
OI Tocheri, Matthew/0000-0001-7600-8998
FU Australian Research Council; Wenner-Gren Foundation
FX Some of the costs associated with analysis of the Liang Bua hominin
remains injakarta were covered by an Australian Research Council grant
to MJM. Conservation efforts were spearheaded by Lorraine Cornish of the
Natural History Museum (London). The Wenner-Gren Foundation provided
funds to support the curation and preservation of the Liang Bua fossil
material. We also thank Djuna Ivereigh (www.indonesiawild.com) for her
photographs of the carpal bones and casts.
NR 23
TC 39
Z9 40
U1 3
U2 23
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0047-2484
J9 J HUM EVOL
JI J. Hum. Evol.
PD NOV
PY 2009
VL 57
IS 5
BP 555
EP 570
DI 10.1016/j.jhevol.2008.06.007
PG 16
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 532XL
UT WOS:000272783600008
PM 19056103
ER
PT J
AU Ram, RS
Yu, S
Gordon, I
Bernath, PF
AF Ram, R. S.
Yu, S.
Gordon, I.
Bernath, P. F.
TI Fourier transform infrared emission spectroscopy of new systems of NiS
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Fourier transform emission spectroscopy; Near infrared spectroscopy;
Rotational analysis; Transition metal sulfides
ID LASER-INDUCED FLUORESCENCE; LOW-LYING STATES; ROTATIONAL ANALYSIS;
EXCITED-STATES; IDENTIFICATION; TRANSITION; NICL; RESOLUTION; SPECTRUM;
OXIDES
AB The emission spectrum of NiS has been investigated in the near infrared in the 2000-7500 cm(-1) region using a Fourier transform spectrometer. New bands observed in the 3000-5000 cm(-1) region have been assigned to a (3)Pi(i)-X(3)Sigma(-) transition analogous to the transition of NiO observed in the near infrared [R.S. Ram and P.F. Bernath, J. Mol. Spectrosc. 155 (1992) 315-325]. The 0-0 band of NiS consists of (3)Pi(0+)-X(3)Sigma(-)(1) (4399 cm(-1)), (3)Pi(0-)-X(3)Sigma(-) (4257 cm(-1)), (3)Pi(1)-X(3)Sigma(-)(0+) (3938 cm(-1)), and (3)Pi(2)-X(3)Sigma(-)(1) (3325 cm(-1)) sub-bands. To higher wavenumbers, another [Omega = 1] - X(3)Sigma(-)(0+) transition has been observed with a 0-0 R head near 5887 cm(-1). This transition has been assigned as (1)Pi-X(3)Sigma(-)(0+), although a (3)Pi(1)-X(3)Sigma(-)(0+) assignment is also possible. Several vibrational bands belonging to different sub-bands were rotationally analyzed and spectroscopic constants evaluated. Our spectroscopic constants for the ground state agree well with the values reported in the microwave Study by Yamamoto et al. [T. Yamamoto, N. Tanimoto, T. Okabayashi. Phys. Chem. Chem. Phys. 9 (2007) 3744-3748]. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Ram, R. S.; Bernath, P. F.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA.
[Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gordon, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bernath, P. F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
RP Ram, RS (reprint author), Univ Arizona, Dept Chem, Room 133,Old Chem Bldg,1306 E Univ Blvd, Tucson, AZ 85721 USA.
EM rram@u.arizona.edu
RI Bernath, Peter/B-6567-2012; Yu, Shanshan/D-8733-2016;
OI Bernath, Peter/0000-0002-1255-396X; Gordon, Iouli/0000-0003-4763-2841
FU NASA; Natural Sciences and Engineering Research Council (NSERC) of
Canada; UK Engineering and Physical Sciences Research Council (EPSRC)
FX The research described here was partially supported by funds from the
NASA laboratory astrophysics program. Some support was also provided by
the Natural Sciences and Engineering Research Council (NSERC) of Canada
and the UK Engineering and Physical Sciences Research Council (EPSRC).
NR 32
TC 1
Z9 1
U1 0
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD NOV-DEC
PY 2009
VL 258
IS 1-2
BP 20
EP 25
DI 10.1016/j.jms.2009.08.013
PG 6
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 528BJ
UT WOS:000272414800004
ER
PT J
AU Yasuhara, M
Cronin, TM
Hunt, G
Hodell, DA
AF Yasuhara, Moriaki
Cronin, Thomas M.
Hunt, Gene
Hodell, David A.
TI DEEP-SEA OSTRACODS FROM THE SOUTH ATLANTIC SECTOR OF THE SOUTHERN OCEAN
DURING THE LAST 370,000 YEARS
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID SUBPOLAR NORTH-ATLANTIC; CLIMATE-CHANGE; PALEOENVIRONMENTAL
IMPLICATIONS; PALAEOCEANOGRAPHICAL CHANGES; SPECIES-DIVERSITY; WATER
CIRCULATION; INDIAN-OCEAN; MAUD RISE; QUATERNARY; ASSEMBLAGES
AB We report changes of deep-sea ostracod fauna during the last 370,000 yr from the Ocean Drilling Program (ODP) Hole 704A in the South Atlantic sector of the Southern Ocean. The results show that faunal changes are coincident with glacial/interglacial-scale deep-water circulation changes, even though our dataset is relatively small and the waters are barren of ostracods until mid-MIS (Marine Isotope Stage) 5. Krithe and Poseidonamicus were dominant during the Holocene interglacial period and the latter part of MIS 5, when this site was under the influence of North Atlantic Deep Water (NADW). Conversely, Henryhowella and Legitimocythere were dominant during glacial periods, when this site was in the path of Circumpolar Deep Water (CPDW). Three new species (Aversovalva brandaoae, Poseidonamicus hisayoae, and Krithe mazziniae) are described herein. This is the first report of Quaternary glacial/interglacial scale deep-sea ostracod faunal changes in the Southern and South Atlantic Oceans, a key region for understanding Quaternary climate and deep-water circulation, although the paucity of Quaternary ostracods in this region necessitates further research.
C1 [Yasuhara, Moriaki; Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Cronin, Thomas M.] US Geol Survey, Reston, VA 20192 USA.
[Hodell, David A.] Univ Cambridge, Dept Earth Sci, Godwin Lab Paleoclimate Res, Cambridge CB2 3EQ, England.
RP Yasuhara, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA.
EM moriakiyasuhara@gmail.com; tcronin@usgs.gov; hunte@si.edu;
dhod07@esc.cam.ac.uk
RI Hunt, Gene/B-3783-2010; Yasuhara, Moriaki/A-4986-2008;
OI Hunt, Gene/0000-0001-6430-5020; Yasuhara, Moriaki/0000-0001-8501-4863;
Yasuhara, Moriaki/0000-0003-0990-1764
FU National Science Foundation; Japan Society; Smithsonian Postdoctoral
Fellowship; Smithsonian Marine Science Network Postdoctoral Fellowship
FX We thank the staff of the U.S. Geological Survey Eastern Earth Surface
Processes Team and the Department of Paleobiology, National Museum of
Natural History, Smithsonian Institution, especially C. Sanford, for
their support throughout this project; H. Okahashi for continuous
support; S. Whittaker for help in SEM imaging; M.Florence for help in
depositing type and figured specimens; K. A. VenZ-CLirtis for help with
samples; S. N. Brandao for taxonomic input; and M. Robinson and J.
Repetski for valuable cornments. This paper benefited from reviews by
two anonymous referees and editing by S. Westrop. This research used
samples provided by the Ocean Drilling Program. The Ocean Drilling
Program is sponsored by the National Science Foundation and
participating countries under the management of Joint Oceanographic
Institutions. This work was supported by the Japan Society for the
Promotion of Science Postdoctoral Fellowships for Research Abroad,
Smithsonian Postdoctoral Fellowship, and Smithsonian Marine Science
Network Postdoctoral Fellowship (to M.Y.).
NR 84
TC 14
Z9 16
U1 2
U2 6
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-3360
EI 1937-2337
J9 J PALEONTOL
JI J. Paleontol.
PD NOV
PY 2009
VL 83
IS 6
BP 914
EP 930
DI 10.1666/08-149.1
PG 17
WC Paleontology
SC Paleontology
GA 522QG
UT WOS:000272012800005
ER
PT J
AU Bernal, XE
Page, RA
Ryan, MJ
Argo, TF
Wilson, PS
AF Bernal, Ximena E.
Page, Rachel A.
Ryan, Michael J.
Argo, Theodore F.
Wilson, Preston S.
TI Acoustic radiation patterns of mating calls of the tungara frog
(Physalaemus pustuosus): Implications for multiple receivers
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID VOCAL SAC; SOUND; VOCALIZATIONS; DIRECTIONALITY; COMMUNICATION;
PARASITOIDS; PUSTULOSUS; TACHINIDAE; PHONOTAXIS; PREDATION
AB In order for a signal to be transmitted from a sender to a receiver, the receiver must be within the active space of the signal. If patterns of sound radiation are not omnidirectional, the position as well as the distance of the receiver relative to the sender is critical. In previous measurements of the horizontal directivity of mating calls of frogs, the signals were analyzed using peak or root-mean-square analysis and resulted in broadband directivities that ranged from negligible to a maximum of approximately 5 dB. Idealized laboratory measurements of the patterns of acoustic radiation of the mating calls of male tungara frogs (Physalaemus pustulosus), along axes relevant to three receivers in this communication network, female frogs in the horizontal plane, and frog-eating bats and blood-sucking flies above the ground, are reported. The highest sound pressure level was radiated directly above the frog, with a 6 dB reduction radiated along the horizontal direction. Band-limited directivities were significantly greater than broadband directivities, with a maximum directivity of 20 dB in the vertical plane for harmonics near 6 kHz. The implications with regard to mating and predator-prey interactions are discussed. (C) 2009 Acoustical Society of America. [DOI: 10.1121/1.3212929]
C1 [Bernal, Ximena E.; Page, Rachel A.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
[Argo, Theodore F.; Wilson, Preston S.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78713 USA.
[Argo, Theodore F.; Wilson, Preston S.] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA.
RP Bernal, XE (reprint author), Texas Tech Univ, Dept Biol Sci, Box 43131, Lubbock, TX 79409 USA.
FU NSF [IBN-0078150]; University of Texas at Austin Cockrell School of
Engineering
FX We thank T. Hollon and K. Miller for their help with frog video
analysis. We appreciate the comments of Michael Owren and one anonymous
reviewer that greatly improved the manuscript. This study was funded by
NSF Grant No. IBN-0078150 and The University of Texas at Austin Cockrell
School of Engineering.
NR 45
TC 4
Z9 4
U1 0
U2 11
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD NOV
PY 2009
VL 126
IS 5
BP 2757
EP 2767
DI 10.1121/1.3212929
PG 11
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA 515XU
UT WOS:000271507000069
PM 19894851
ER
PT J
AU MacKay, MD
Neale, PJ
Arp, CD
Domis, LND
Fang, X
Gal, G
Johnk, KD
Kirillin, G
Lenters, JD
Litchman, E
MacIntyre, S
Marsh, P
Melack, J
Mooij, WM
Peeters, F
Quesada, A
Schladow, SG
Schmid, M
Spence, C
Stokesr, SL
AF MacKay, M. D.
Neale, P. J.
Arp, C. D.
Domis, L. N. De Senerpont
Fang, X.
Gal, G.
Joehnk, K. D.
Kirillin, G.
Lenters, J. D.
Litchman, E.
MacIntyre, S.
Marsh, P.
Melack, J.
Mooij, W. M.
Peeters, F.
Quesada, A.
Schladow, S. G.
Schmid, M.
Spence, C.
Stokesr, S. L.
TI Modeling lakes and reservoirs in the climate system
SO LIMNOLOGY AND OCEANOGRAPHY
LA English
DT Review
ID NORTH-ATLANTIC OSCILLATION; SHALLOW LAKES; LONG-TERM; EUROPEAN LAKES;
BOREAL LAKES; GREAT-LAKES; AQUATIC ECOSYSTEM; WATER TEMPERATURE;
MIDSUMMER DECLINE; PLANKTON DYNAMICS
AB Modeling studies examining the effect of lakes on regional and global climate, as well as studies on the influence of climate variability and change on aquatic ecosystems, are surveyed. Fully coupled atmosphere-land surface-lake climate models that could be used for both of these types of study simultaneously do not presently exist, though there are many applications that would benefit from such models. It is argued here that current understanding of physical and biogeochemical processes in freshwater systems is sufficient to begin to construct such models, and a path forward is proposed. The largest impediment to fully representing lakes in the climate system lies in the handling of lakes that are too small to be explicitly resolved by the climate model, and that make up the majority of the lake-covered area at the resolutions currently used by global and regional climate models. Ongoing development within the hydrological sciences community and continual improvements in model resolution should help ameliorate this issue.
C1 [MacKay, M. D.] Environm Canada, Div Climate Res, Toronto, ON, Canada.
[Neale, P. J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Arp, C. D.] US Geol Survey, Anchorage, AK USA.
[Domis, L. N. De Senerpont; Mooij, W. M.] Ctr Limnol, Dept Aquat Food Webs, Nieuwersluis, Netherlands.
[Fang, X.] Auburn Univ, Dept Civil Engn, Auburn, AL 36849 USA.
[Gal, G.] Israel Oceanog & Limnol Res, Kinneret Limnol Lab, Migdal, Israel.
[Joehnk, K. D.] Leibniz Inst Freshwater Ecol & Inland Fisheries, Dept Limnol Stratified Lakes, Neuglobsow, Germany.
[Kirillin, G.] Leibniz Inst Freshwater Ecol & Inland Fisheries, Dept Ecohydrol, Berlin, Germany.
[Lenters, J. D.] Univ Nebraska, Sch Nat Resources, Lincoln, NE USA.
[Litchman, E.] Michigan State Univ, WK Kellogg Biol Stn, Hickory Corners, MI 49060 USA.
[MacIntyre, S.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Marsh, P.; Spence, C.] Environm Canada, Natl Hydrol Res Ctr, Saskatoon, SK, Canada.
[Melack, J.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Peeters, F.] Univ Konstanz, Limnol Inst, Dept Biol, Constance, Germany.
[Quesada, A.] Univ Autonoma Madrid, Dept Biol, Madrid, Spain.
[Schladow, S. G.] Univ Calif Davis, Tahoe Environm Res Ctr, Davis, CA USA.
[Schmid, M.] Eawag Swiss Fed Inst Aquat Sci & Technol Surface, Kastanienbaum, Switzerland.
[Stokesr, S. L.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
RP MacKay, MD (reprint author), Environm Canada, Div Climate Res, Toronto, ON, Canada.
EM murray.mackay@ec.gc.ca
RI Schmid, Martin/C-3953-2009; De Senerpont Domis, Lisette/C-2902-2008;
Kirillin, Georgiy/B-5410-2010; Neale, Patrick/A-3683-2012; Mooij,
Wolf/C-2677-2008; Johnk, Klaus/B-3382-2008
OI Schmid, Martin/0000-0001-8699-5691; Quesada,
Antonio/0000-0002-8913-5993; De Senerpont Domis,
Lisette/0000-0001-7509-9541; Kirillin, Georgiy/0000-0001-7337-3586;
Mooij, Wolf/0000-0001-5586-8200; Johnk, Klaus/0000-0002-5972-4201
FU Ministerio de Educacion y Ciencia (Spain) [CGL2005-06549-CO2-01];
Smithsonian Institution; NSF Division of Environmental Biology
[0552283]; Earth and Life Science Foundation (ALW) [817.01.007];
Netherlands Organization for Scientific Research (NWO)
FX A. Q. was supported by Ministerio de Educacion y Ciencia (Spain) with
grant CGL2005-06549-CO2-01; P. J. N. was supported by the Smithsonian
Institution and NSF Division of Environmental Biology grant 0552283; and
L. d. S. D. and W. M. M. were supported by grant 817.01.007 of the Earth
and Life Science Foundation (ALW), which is subsidized by the
Netherlands Organization for Scientific Research (NWO).
NR 162
TC 41
Z9 44
U1 3
U2 44
PU AMER SOC LIMNOLOGY OCEANOGRAPHY
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA
SN 0024-3590
J9 LIMNOL OCEANOGR
JI Limnol. Oceanogr.
PD NOV
PY 2009
VL 54
IS 6
BP 2315
EP 2329
DI 10.4319/lo.2009.54.6_part_2.2315
PN 2
PG 15
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 532YC
UT WOS:000272785700004
ER
PT J
AU Sobrino, C
Neale, PJ
Phillips-Kress, JD
Moeller, RE
Porter, JA
AF Sobrino, Cristina
Neale, P. J.
Phillips-Kress, J. D.
Moeller, R. E.
Porter, J. A.
TI Elevated CO2 increases sensitivity to ultraviolet radiation in
lacustrine phytoplankton assemblages
SO LIMNOLOGY AND OCEANOGRAPHY
LA English
DT Article
ID DISSOLVED ORGANIC-MATTER; INORGANIC CARBON; FRESH-WATER; CLIMATE-CHANGE;
UV-RADIATION; DNA-DAMAGE; PHOTOSYNTHESIS; LAKES; INHIBITION;
CYANOBACTERIA
AB This study tests the effects of elevated CO2 and ultraviolet radiation (UVR) on phytoplankton photosynthesis through in situ incubations in Lake Giles, Pennsylvania. In a first experiment, CO2 was supplied from a tank to simulate atmospheric CO2 concentrations predicted in scenarios of future global change. In a second experiment, elevated CO2 conditions were obtained by the mineralization of added colored dissolved organic matter (CDOM) of terrestrial origin (400 mmol L-1 final concentration). The results demonstrated that for natural assemblages from Lake Giles, atmospheric CO2 concentrations similar to those predicted for the end of the century can increase primary productivity up to 23% in the absence of photoinhibition. However, elevated CO2 concentrations also increased sensitivity of phytoplankton to UVR, making cells more susceptible and increasing photoinhibition. Increased sensitivity was observed in samples incubated with the artificial CO2 supply as well as with the CDOM addition, the latter resulting in CO2 partial pressures close to three times present atmospheric levels. Photosynthetic rate modeled for elevated CO2 and midday solar exposure just below the lake surface was 17% of potential production compared with 21% under usual CO2 levels in the lake, resulting in similar rates between phytoplankton assemblages grown under high and low CO2 levels. Understanding the effect on primary productivity of the interaction between factors that may be affected by global change is essential to predict future changes in ecosystems and climate.
C1 [Sobrino, Cristina; Neale, P. J.; Phillips-Kress, J. D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Moeller, R. E.] Miami Univ, Oxford, OH 45056 USA.
[Porter, J. A.] Lehigh Univ, Bethlehem, PA 18015 USA.
RP Sobrino, C (reprint author), Univ Vigo, Vigo 36310, Spain.
EM sobrinoc@uvigo.es
RI Neale, Patrick/A-3683-2012;
OI Sobrino, Cristina/0000-0003-0431-1220
FU Spanish Ministry of Education and Science; Smithsonian Institution;
National Science Foundation [DEB-IRCEB-0552283]
FX We thank the Lacawac Sanctuary for use of its facilities, and the
Blooming Grove Hunting and Fishing Club for access to Lake Giles. Donald
Morris (Lehigh) devised the CDOM concentrating protocol, and Craig
Williamson (Miami) provided light and UV attenuation data for Lake
Giles. We also thank two anonymous reviewers for their suggestions on
the previous version of this manuscript.; This research was supported by
postdoctoral fellowships to C. S. from the Spanish Ministry of Education
and Science and from the Smithsonian Institution, and by National
Science Foundation grant DEB-IRCEB-0552283.
NR 47
TC 23
Z9 23
U1 1
U2 16
PU AMER SOC LIMNOLOGY OCEANOGRAPHY
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA
SN 0024-3590
J9 LIMNOL OCEANOGR
JI Limnol. Oceanogr.
PD NOV
PY 2009
VL 54
IS 6
BP 2448
EP 2459
DI 10.4319/lo.2009.54.6_part_2.2448
PN 2
PG 12
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 532YC
UT WOS:000272785700013
ER
PT J
AU O'Connor, KA
Ferrell, R
Brindle, E
Trumble, B
Shofer, J
Holman, DJ
Weinstein, M
AF O'Connor, Kathleen A.
Ferrell, Rebecca
Brindle, Eleanor
Trumble, Benjamin
Shofer, Jane
Holman, Darryl J.
Weinstein, Maxine
TI Progesterone and ovulation across stages of the transition to menopause
SO MENOPAUSE-THE JOURNAL OF THE NORTH AMERICAN MENOPAUSE SOCIETY
LA English
DT Article
DE Pregnanediol glucuronide; Urinary hormones; Menopause; Perimenopause;
Reproductive aging; Reproductive stage; Follicle-stimulating hormone;
Luteinizing hormone; Estrone glucuronide; Anovulation
ID HUMAN MENSTRUAL-CYCLE; REPRODUCTIVE HORMONES; LUTEINIZING-HORMONE;
POPULATION-RESEARCH; BLEEDING CRITERIA; OVARIAN-FUNCTION; LUTEAL
FUNCTION; BREAST-CANCER; OLDER WOMEN; BODY-SIZE
AB Objective: Detailed characterization of progesterone and ovulation across the menopausal transition provides insight into conception risk and mechanisms of reproductive aging.
Methods: Participants (n = 108, aged 25-58 y) collected daily urine specimens for 6-month intervals in each of 5 consecutive years. Specimens were assayed for pregnanediol glucuronide (PDG), luteinizing hormone (LH), follicle-stimulating hormone (FSH), and estrone glucuronide (EIG). Reproductive stage was determined using cycle length variance. A hierarchical algorithm was used to identify ovulation. Linear mixed-effects models estimated (1) the frequency and day of ovulation by age and stage; (2) differences in FSH, LH, and E I G levels between ovulatory (0) and anovulatory (AO) cycles; and (3) total PDG levels and PDG levels in 0 cycles by age and stage.
Results: The probability of AO cycles increased across the perimenopause (P < 0.0001); reproductive stage was a stronger predictor than age of the probability of anovulation. Most cycles in late perimenopause were AO (>60%), but one quarter of cycles longer than 60 days were O. Average day of ovulation was later in the late perimenopause (mean [SD] cycle day, 27 [25] d) compared with the premenopause. FSH and LH levels were higher and EIG levels were lower in AO than O cycles (P < 0.0001 for each). Total PDG decreased in the late perimenopause, but 95th percentile PDG in 0 cycles declined steadily across the transition.
Conclusions: Exposure to the risk of conception in women experiencing cycles long enough to classify them as late perimenopausal is far from negligible. Reproductive stage is more informative than age about PDG levels and the likelihood of anovulation.
C1 [O'Connor, Kathleen A.; Trumble, Benjamin; Holman, Darryl J.] Univ Washington, Dept Anthropol, Seattle, WA 98195 USA.
[O'Connor, Kathleen A.; Brindle, Eleanor; Trumble, Benjamin; Shofer, Jane; Holman, Darryl J.] Univ Washington, Ctr Studies Demog & Ecol, Seattle, WA 98195 USA.
[Ferrell, Rebecca] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA.
[Weinstein, Maxine] Georgetown Univ, Ctr Populat & Hlth, Washington, DC USA.
RP O'Connor, KA (reprint author), Univ Washington, Dept Anthropol, Box 353100, Seattle, WA 98195 USA.
EM oconnork@u.washington.edu
OI Brindle, Eleanor/0000-0002-4272-0909
FU Population Research Institute of Pennsylvania State University; Center
for Studies in Demography and Ecology of the University of Washington;
Center for Population and Health, Georgetown University; National
Institute on Aging (NIA) [RO1 AG15141, NIA 5 T32 AG00208]; National
Institute of Child Health and Development (NICHD) [HD34159, NICHD 2 P30
HD28263, NICHD F32 HD 07994-02, NICHD 5 T32 HD007543-07]
FX This research was partly supported by the Population Research Institute
of Pennsylvania State University, the Center for Studies in Demography
and Ecology of the University of Washington, and the Center for
Population and Health, Georgetown University, as well as by the
following grants: National Institute on Aging (NIA) RO1 AG15141, NIA 5
T32 AG00208, National Institute of Child Health and Development (NICHD)
HD34159, NICHD 2 P30 HD28263, NICHD F32 HD 07994-02, and NICHD 5 T32
HD007543-07.
NR 60
TC 29
Z9 30
U1 2
U2 5
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 1072-3714
EI 1530-0374
J9 MENOPAUSE
JI Menopause-J. N. Am. Menopause Soc.
PD NOV-DEC
PY 2009
VL 16
IS 6
BP 1178
EP 1187
DI 10.1097/gme.0b013e3181aa192d
PG 10
WC Obstetrics & Gynecology
SC Obstetrics & Gynecology
GA 518ZB
UT WOS:000271733700018
PM 19568209
ER
PT J
AU Kapheim, KM
Pollinger, JP
Wcislo, WT
Wayne, RK
AF Kapheim, Karen M.
Pollinger, John P.
Wcislo, William T.
Wayne, Robert K.
TI Characterization of 12 polymorphic microsatellite markers for a
facultatively eusocial sweat bee (Megalopta genalis)
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE eusociality; Halictidae; Megalopta genalis; microsatellite; molecular
marker; relatedness
ID ECUADORIA HYMENOPTERA; HALICTIDAE; EVOLUTION
AB We developed a library of twelve polymorphic di- and tri-nucleotide microsatellite markers for Megalopta genalis, a facultatively eusocial sweat bee. We tested each locus in a panel of 23 unrelated females and found 7-20 alleles per locus. Observed and expected heterozygosities ranged from 0.65 to 0.96 and from 0.69 to 0.95 respectively. None of the loci deviated from Hardy-Weinberg equilibrium proportions or was found to be in gametic disequilibrium.
C1 [Kapheim, Karen M.; Pollinger, John P.; Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Kapheim, KM (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr S, Los Angeles, CA 90095 USA.
EM kapheimk@ucla.edu
FU Smithsonian Tropical Research Institute; U. S. Department of Education;
UCLA EEB
FX We thank Adam Smith, Margarita Lopez-Uribe, Julian Medina-Gutierrez,
Dyana LaRosa, Ricardo Cossio, & Michael Reiser for field assistance, and
the Autoridad Nacional del Ambiente of the Republic of Panama for
permission to export specimens. Partial field work support was provided
by general research funds from the Smithsonian Tropical Research
Institute (WTW), a Smithsonian Tropical Research Institute Short-term
Fellowship (KMK), a U. S. Department of Education GAANN fellowship
(KMK), and a Holmes O. Miller Fellowship from UCLA EEB (KMK).
NR 14
TC 4
Z9 4
U1 0
U2 2
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD NOV
PY 2009
VL 9
IS 6
BP 1527
EP 1529
DI 10.1111/j.1755-0998.2009.02693.x
PG 3
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 506PK
UT WOS:000270787500021
PM 21564949
ER
PT J
AU Sanin, C
Cadena, CD
Maley, JM
Lijtmaer, DA
Tubaro, PL
Chesser, RT
AF Sanin, Camilo
Daniel Cadena, Carlos
Maley, James M.
Lijtmaer, Dario A.
Tubaro, Pablo L.
Chesser, R. Terry
TI Paraphyly of Cinclodes fuscus (Aves: Passeriformes: Furnariidae):
Implications for taxonomy and biogeography
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Andes; Patagonia; Phylogeography; Species limits; Bar-winged Cinclodes
ID OVENBIRD GENUS CINCLODES; GEOGRAPHIC RANGE; MITOCHONDRIAL-DNA; ANCESTRAL
AREAS; EVOLUTION; BIRDS; SYSTEMATICS; SPECIATION; TYRANTS; FOREST
AB The Andes are a hotspot of global avian diversity, but studies on the historical diversification of Andean birds remain relatively scarce. Evolutionary studies on avian lineages with Andean-Patagonian distributions have focused on reconstructing species-level phylogenies, whereas no detailed phylogeographic studies on widespread species have been conducted. Here, we describe phylogeographic patterns in the Bar-winged Cinclodes (Cinclodes fuscus), a widespread and common species of ovenbird (Furnariidae) that breeds from Tierra del Fuego to the northern Andes. Traditionally, C. fuscus has been considered a single species composed of nine subspecies, but its long and narrow range suggests the possibility of considerable genetic variation among populations. Sequences of two mitochondrial genes revealed three discrete and geographically coherent groups of C. fuscus, occupying the southern, central, and northern Andes. Surprisingly, phylogenetic analyses indicated that these groups were more closely related to other species of Cinclodes than to each other. Relationships of the southern and northern C. fuscus clades to other species of Cinclodes were straightforward; in combination with available information on plumage, behavioral, and vocal variation, this suggests that each should be recognized as a distinct biological species. The central Andean group was paraphyletic with respect to C. oustaleti, and relationships among these taxa and C. olrogi were poorly resolved. We suggest that the central Andean C. fuscus should also be considered a different species, pending new information to clarify species limits in this group. These new phylogenetic data, along with recently developed methods, allowed us to review the biogeography of the genus, confirming southern South America and the central Andes as important areas for the diversification of these birds. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Sanin, Camilo] Univ Los Andes, Dept Ciencias Biol, Lab Biol Evolut Vertebrados, Bogota 4976, Colombia.
[Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
[Maley, James M.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Maley, James M.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Lijtmaer, Dario A.; Tubaro, Pablo L.] Museo Argentino Ciencias Nat Bernardino Rivadavia, Div Ornitol, Buenos Aires, DF, Argentina.
RP Sanin, C (reprint author), Univ Los Andes, Dept Ciencias Biol, Lab Biol Evolut Vertebrados, Apartado Aereo, Bogota 4976, Colombia.
EM ca-sanin@uniandes.edu.co; ccadena@uniandes.edu.co; jmaley1@lsu.edu;
dlijtmaer@macn.gov.ar; ptubaro@interlink.com.ar; chessert@si.edu
RI Cadena, Carlos Daniel/G-1313-2010
FU RTP, M. Sangrey; Robert Fri Internship Endowment; National Museum of
Natural History; ADRC; Department of Vertebrate Zoology; Frank M.
Chapman Memorial Fund; American Museum of Natural History; NSF
[DBI-0400797, DEB-0543562, IOS-0848028]; Facultad de Ciencias,
Universidad de los Andes
FX This study originated as a Smithsonian Research Training Program (RTP)
internship project conducted by CS with RTC. We thank the RTP, M.
Sangrey and the Robert Fri Internship Endowment for their support of the
project. The project received additional financial support from the
National Museum of Natural History; we thank H. Sues and W. Wiswall of
the office of the ADRC and R. Vari of the Department of Vertebrate
Zoology for providing funding for molecular labwork at the Smithsonian.
We are grateful to R.C. Fleischer for providing access to the laboratory
facilities at the Genetics Lab of the National Zoological Park,
Smithsonian Institution; and to N. Rotzel, S. Haas, J. Maldonado and E.
Latch for their assistance in the laboratory. Labwork at LSU was
supported by a grant from the Frank M. Chapman Memorial Fund, American
Museum of Natural History, to JMM and in part by NSF Grants DBI-0400797
and DEB-0543562 to R. T. Brumfield. Amplification and sequencing of the
specimen from Colombia were funded by the Facultad de Ciencias,
Universidad de los Andes through a grant to CDC. Additional support for
this project was provided by NSF Grant IOS-0848028 to C. Martinez del
Rio. We thank M. Nores and A. Jaramillo for their comments during
preparation of the manuscript, and J. Klicka, M. A. Aponte and J. A.
Gerwin for information about certain specimens. We thank the following
for contributing tissue samples or sequences to this project: J. Bates
and D. Willard, Field Museum of Natural History, Chicago; S. Birks,
Burke Museum, University of Washington, Seattle; N. Rice, Academy of
Natural Sciences, Philadelphia; and J. Avendano and A. Navas, Museo de
Historia Natural ANDES, Colombia. RTC thanks T. Valqui, A. Urbay, D.
Susanibar, P. Sweet, C. Kovacs and son, "Checho" Escobar, and A. Pena
for assistance with logistics and fieldwork, and the following
individuals and institutions for kindly granting collecting and export
permits for their jurisdictions: A. Morizaki Taura, Instituto Nacional
de Recursos Naturales (INRENA), Lima, Peru; M. Etchegoin, Direccion de
Recursos Naturales Renovables, Provincia de Cordoba, Cordoba, Argentina;
R. Lini, Direccion de Bosques y Fauna, Provincia de Rio Negro, Viedma,
Argentina; G. Porini, Secretaria de Recursos Naturales y Ambiente
Humano, Buenos Aires, Argentina; and J. C. Cuchacovich, Servicio
Agricola y Ganadero, Santiago, Chile. Any use of trade, product, or firm
names is for descriptive purposes only and does not imply endorsement by
the U.S. Government.
NR 49
TC 19
Z9 20
U1 0
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD NOV
PY 2009
VL 53
IS 2
BP 547
EP 555
DI 10.1016/j.ympev.2009.06.022
PG 9
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 547MD
UT WOS:000273892200017
PM 19580881
ER
PT J
AU Camargo, A
Heyer, WR
de Sa, RO
AF Camargo, Arley
Heyer, W. Ronald
de Sa, Rafael O.
TI Phylogeography of the frog Leptodactylus validus (Amphibia: Anura):
Patterns and timing of colonization events in the Lesser Antilles
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Biogeography; West Indies; Mitochondrial DNA; Phylogeography; Dating;
Coalescent; Leptodactylus
ID WEST-INDIAN VERTEBRATES; STATISTICAL PHYLOGEOGRAPHY;
GEOGRAPHICAL-DISTRIBUTION; CLADISTIC-ANALYSIS; FAILS CONTINUE;
POPULATION; BIOGEOGRAPHY; HAPLOTYPES; INFERENCE; COALESCENT
AB The frog Leptodactylus validus occurs in northern South America, Trinidad and Tobago, and the southern Lesser Antilles (Grenada and St. Vincent). Mitochondrial DNA sequences were used to perform a nested clade phylogeographic analysis (NCPA), to date colonization events, and to analyze colonization patterns using on a relaxed molecular clock and coalescent simulations. L. validus originated on the mainland and first colonized Trinidad with subsequent independent colonizations of Tobago and the Lesser Antilles from Trinidad. The NCPA suggests a historical vicariant event between populations in Trinidad and Tobago from those in the Lesser Antilles. The colonization of Trinidad occurred similar to 1 million years ago (mya) and the colonization of the Lesser Antillean islands occurred similar to 0.4 mya. The coalescent approach supported the scenario where L. validus dispersed from Trinidad to St. Vincent and from there to Grenada, a dispersal event that could have been mediated by human introduction as recent as 1600 years ago. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Camargo, Arley] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA.
[de Sa, Rafael O.] Univ Richmond, Dept Biol, Richmond, VA 23173 USA.
[Heyer, W. Ronald] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP Camargo, A (reprint author), Brigham Young Univ, Dept Biol, 177 WIDB, Provo, UT 84602 USA.
EM arley.camargo@gmail.com
RI Camargo Bentaberry, Arley/A-2975-2008
OI Camargo Bentaberry, Arley/0000-0001-7734-8679
FU National Science Foundation [0342918]
FX R.O. de Sa and W.R. Heyer acknowledge funding support for this study
through National Science Foundation award # 0342918. We thank two
anonymous reviewers whose comments and suggestions improved an earlier
version of the manuscript.
NR 50
TC 11
Z9 12
U1 2
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
EI 1095-9513
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD NOV
PY 2009
VL 53
IS 2
BP 571
EP 579
DI 10.1016/j.ympev.2009.07.004
PG 9
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 547MD
UT WOS:000273892200020
PM 19596454
ER
PT J
AU Vergara-Chen, C
Aguirre, WE
Gonzalez-Wanguemert, M
Bermingham, E
AF Vergara-Chen, Carlos
Aguirre, Windsor E.
Gonzalez-Wanguemert, Mercedes
Bermingham, Eldredge
TI A mitochondrial DNA based phylogeny of weakfish species of the Cynoscion
group (Pisces: Sciaenidae)
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE ATPase 8/6; Atractoscion; Cynoscion; Cytochrome b; Geminate species;
Isopisthus; Molecular systematics; Macrodon; Plagioscion
ID PERCIFORMES; ECUADOR; GULF
AB We infer the phylogeny of fishes in the New World Cynoscion group (Cynoscion, Isopisthus, Macrodon, Atractoscion, Plagioscion) using 1603 bp of DNA sequence data from three mitochondrial genes. With the exception of Plagioscion, whose position was ambiguous, the Cynoscion group is monophyletic. However, several genera examined are not monophyletic. Atlantic and Pacific species of Cynoscion are interspersed in the tree and geminate species pairs are identified. Intergeneric relationships in the group are clarified. Our analysis is the first comprehensive phylogeny for the Cynoscion group based on molecular data and provides a baseline for future comparative studies of this important group. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Vergara-Chen, Carlos; Gonzalez-Wanguemert, Mercedes] Univ Murcia, Dept Ecol & Hidrol, Fac Biol, E-30100 Murcia, Spain.
[Aguirre, Windsor E.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA.
[Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Vergara-Chen, C (reprint author), Univ Murcia, Dept Ecol & Hidrol, Fac Biol, Campus Espinardo, E-30100 Murcia, Spain.
EM carlos.vergara@alu.um.es; windsor.aguirre@gmail.com; mergonza@um.es;
bermingham@si.edu
RI Gonzalez-Wanguemert, Mercedes/M-3467-2013;
OI Gonzalez-Wanguemert, Mercedes/0000-0002-0656-358X; Vergara-Chen,
Carlos/0000-0002-6314-3231
FU Corporacion Elektra Noreste; Smithsonian Tropical Research Institute;
American Museum of Natural History
FX The authors thank the governmental authorities of Panama, Ecuador,
Venezuela, Mexico, and the United States for permits and support of our
research. For assistance obtaining samples we thank Martha
Roman-Rodriguez, Manuel Grijalva-Chon, Thomas Orrel, Javier Jara, Felix
Rodriguez, Alejandra Volpedo, Orangel Aguilera, Tim Targett, Jeanne
Boylan, Robert McMichael, Debbie Leffler, Butch Pellegrin, Larry Allen,
Dan Pondella, and Mike Shane. CVC was supported by a research grant from
the Corporacion Elektra Noreste and the Smithsonian Tropical Research
Institute. Richard Cooke, Ricardo Betancur, Andrew Crawford and John J.
Wiens' Lab provided helpful comments on the manuscript. WEA is grateful
for support from Ken Stuck, Walter Grater, Stuart Poss, R. Geeta,
Michael A. Bell and funding from a Lerner-Gray Grant (American Museum of
Natural History).
NR 18
TC 10
Z9 15
U1 0
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD NOV
PY 2009
VL 53
IS 2
BP 602
EP 607
DI 10.1016/j.ympev.2009.06.013
PG 6
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 547MD
UT WOS:000273892200024
PM 19573613
ER
PT J
AU Nardini, E
Risaliti, G
Salvati, M
Sani, E
Watabe, Y
Marconi, A
Maiolino, R
AF Nardini, E.
Risaliti, G.
Salvati, M.
Sani, E.
Watabe, Y.
Marconi, A.
Maiolino, R.
TI Exploring the active galactic nucleus and starburst content of local
ultraluminous infrared galaxies through 5-8 mu m spectroscopy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: starburst; infrared: galaxies
ID SPITZER-SPACE-TELESCOPE; POLYCYCLIC AROMATIC-HYDROCARBONS; INTERSTELLAR
EXTINCTION LAW; PALOMAR-GREEN QUASARS; COMPTON-THICK AGN; X-RAY SURVEY;
XMM-NEWTON; STAR-FORMATION; MIDINFRARED SPECTROSCOPY; OPTICAL
SPECTROSCOPY
AB We present a 5-8 mu m analysis of the Spitzer spectra of 71 ultraluminous infrared galaxies (ULIRGs) with redshift z < 0.15, devoted to the study of the role of active galactic nuclei (AGN) and starbursts (SBs) as the power source of the extreme infrared emission. Around similar to 5 mu m, an AGN is much brighter (by a factor of approximate to 30) than an SB of equal bolometric luminosity. This allows us to detect the presence of even faint accretion-driven cores inside ULIRGs: signatures of AGN activity are found in similar to 70 per cent of our sample (50/71 sources). Through a simple analytical model, we are also able to obtain a quantitative estimate of the AGN/SB contribution to the overall energy output of each source. Although the main fraction of ULIRG luminosity is confirmed to arise from star formation events, the AGN contribution is non-negligible (similar to 23 per cent) and is shown to increase with luminosity. The existence of a rather heterogeneous pattern in the composition and geometrical structure of the dust among ULIRGs is newly supported by the comparison between individual absorption features and continuum extinction.
C1 [Nardini, E.; Sani, E.; Marconi, A.] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy.
[Risaliti, G.; Salvati, M.; Watabe, Y.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Maiolino, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
RP Nardini, E (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Lgo E Fermi 2, I-50125 Florence, Italy.
EM nardini@arcetri.astro.it
RI Marconi, Alessandro/C-5880-2009;
OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti,
Guido/0000-0002-3556-977X
FU Jet Propulsion Laboratory; California Institute of Technology; National
Aeronautics and Space Administration; PRIN-MIUR [2006025203]; ASI-INAF
[I/088/06/0, I/016/07/0]
FX We are grateful to the anonymous referee for the constructive comments
and suggestions that improved our work. This research has made use of
the NASA/IPAC Extragalactic Data base which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. We
acknowledge financial support from PRIN-MIUR 2006025203 grant, and from
ASI-INAF I/088/06/0 and ASI-INAF I/016/07/0 contracts.
NR 98
TC 31
Z9 31
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV 1
PY 2009
VL 399
IS 3
BP 1373
EP 1402
DI 10.1111/j.1365-2966.2009.15357.x
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508BP
UT WOS:000270902100022
ER
PT J
AU Guffanti, M
Mayberry, GC
Casadevall, TJ
Wunderman, R
AF Guffanti, Marianne
Mayberry, Gari C.
Casadevall, Thomas J.
Wunderman, Richard
TI Volcanic hazards to airports
SO NATURAL HAZARDS
LA English
DT Article
DE Volcanic hazards; Volcanic ash; Airports; Volcanic-risk mitigation
ID WEATHER RADAR; ASH; ERUPTION; ISLANDS; CLOUD
AB Volcanic activity has caused significant hazards to numerous airports worldwide, with local to far-ranging effects on travelers and commerce. Analysis of a new compilation of incidents of airports impacted by volcanic activity from 1944 through 2006 reveals that, at a minimum, 101 airports in 28 countries were affected on 171 occasions by eruptions at 46 volcanoes. Since 1980, five airports per year on average have been affected by volcanic activity, which indicates that volcanic hazards to airports are not rare on a worldwide basis. The main hazard to airports is ashfall, with accumulations of only a few millimeters sufficient to force temporary closures of some airports. A substantial portion of incidents has been caused by ash in airspace in the vicinity of airports, without accumulation of ash on the ground. On a few occasions, airports have been impacted by hazards other than ash (pyroclastic flow, lava flow, gas emission, and phreatic explosion). Several airports have been affected repeatedly by volcanic hazards. Four airports have been affected the most often and likely will continue to be among the most vulnerable owing to continued nearby volcanic activity: Fontanarossa International Airport in Catania, Italy; Ted Stevens Anchorage International Airport in Alaska, USA; Mariscal Sucre International Airport in Quito, Ecuador; and Tokua Airport in Kokopo, Papua New Guinea. The USA has the most airports affected by volcanic activity (17) on the most occasions (33) and hosts the second highest number of volcanoes that have caused the disruptions (5, after Indonesia with 7). One-fifth of the affected airports are within 30 km of the source volcanoes, approximately half are located within 150 km of the source volcanoes, and about three-quarters are within 300 km; nearly one-fifth are located more than 500 km away from the source volcanoes. The volcanoes that have caused the most impacts are Soufriere Hills on the island of Montserrat in the British West Indies, Tungurahua in Ecuador, Mt. Etna in Italy, Rabaul caldera in Papua New Guinea, Mt. Spurr and Mt. St. Helens in the USA, Ruapehu in New Zealand, Mt. Pinatubo in the Philippines, and Anatahan in the Commonwealth of the Northern Mariana Islands (part of the USA). Ten countries-USA, Indonesia, Ecuador, Papua New Guinea, Italy, New Zealand, Philippines, Mexico, Japan, and United Kingdom-have the highest volcanic hazard and/or vulnerability measures for airports. The adverse impacts of volcanic eruptions on airports can be mitigated by preparedness and forewarning. Methods that have been used to forewarn airports of volcanic activity include real-time detection of explosive volcanic activity, forecasts of ash dispersion and deposition, and detection of approaching ash clouds using ground-based Doppler radar. Given the demonstrated vulnerability of airports to disruption from volcanic activity, at-risk airports should develop operational plans for ashfall events, and volcano-monitoring agencies should provide timely forewarning of imminent volcanic-ash hazards directly to airport operators.
C1 [Guffanti, Marianne] US Geol Survey, Reston, VA 20192 USA.
[Mayberry, Gari C.] US Geol Survey, Washington, DC 20560 USA.
[Casadevall, Thomas J.] US Geol Survey, Denver, CO 80225 USA.
[Wunderman, Richard] Smithsonian Inst, Washington, DC 20560 USA.
RP Guffanti, M (reprint author), US Geol Survey, Reston, VA 20192 USA.
EM guffanti@usgs.gov
FU USGS Volcano Hazards Program
FX This work was supported by the USGS Volcano Hazards Program. Chris
Newhall, Steve Brantley, and two anonymous reviewers provided helpful
reviews of this report.
NR 35
TC 40
Z9 41
U1 4
U2 29
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
J9 NAT HAZARDS
JI Nat. Hazards
PD NOV
PY 2009
VL 51
IS 2
BP 287
EP 302
DI 10.1007/s11069-008-9254-2
PG 16
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 501ML
UT WOS:000270385900005
ER
PT J
AU Boukobza, E
Cohen, D
Vardi, A
AF Boukobza, Erez
Cohen, Doron
Vardi, Amichay
TI Interaction-induced dynamical phase locking of Bose-Einstein condensates
SO PHYSICAL REVIEW A
LA English
DT Article
DE Bose-Einstein condensation; quantum optics
ID QUANTUM PHASE; JOSEPHSON-JUNCTION; INTERFERENCE; ATOMS; STATE;
TRANSITION; DIFFUSION; COHERENCE; NUMBER; GASES
AB We show that interactions result in the emergence of a definite relative phase between two initially incoherent Bose-Einstein condensates. The many-realization interference fringe visibility is universal at g(12)((1))similar to 1/3 throughout the Josephson interaction regime as evident from a semiclassical picture. Other types of incoherent preparation yield qualitatively different coherence dynamics.
C1 [Boukobza, Erez; Vardi, Amichay] Ben Gurion Univ Negev, Dept Chem, IL-84105 Beer Sheva, Israel.
[Cohen, Doron] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel.
[Vardi, Amichay] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Boukobza, E (reprint author), Ben Gurion Univ Negev, Dept Chem, POB 653, IL-84105 Beer Sheva, Israel.
RI Vardi, Amichay/D-8189-2011; Cohen, Doron/D-4564-2009
OI Vardi, Amichay/0000-0002-8992-2129; Cohen, Doron/0000-0002-3835-3544
FU Israel Science Foundation [582/07]; United States-Israel Binational
Science Foundation (BSF) [2006021, 2008141]; National Science Foundation
FX This work was supported by the Israel Science Foundation (Grant No.
582/07), by Grants No. 2006021 and No. 2008141 from the United
States-Israel Binational Science Foundation (BSF), and by the National
Science Foundation through a grant for the Institute for Theoretical
Atomic, Molecular, and Optical Physics at Harvard University and
Smithsonian Astrophysical Observatory.
NR 37
TC 6
Z9 6
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD NOV
PY 2009
VL 80
IS 5
AR 053619
DI 10.1103/PhysRevA.80.053619
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 526RH
UT WOS:000272310000139
ER
PT J
AU Ticknor, C
AF Ticknor, Christopher
TI Two-dimensional dipolar scattering
SO PHYSICAL REVIEW A
LA English
DT Article
DE intermolecular mechanics; molecular moments; scattering; wave functions
ID 2 DIMENSIONS; GAS
AB We characterize the long-range dipolar scattering in two dimensions. We use the analytic zero energy wave function including the dipolar interaction; this solution yields universal dipolar scattering properties in the threshold regime. We also study the semiclassical dipolar scattering and find universal dipolar scattering for this energy regime. For both energy regimes, we discuss the validity of the universality and give physical examples of the scattering.
C1 [Ticknor, Christopher] Swinburne Univ Technol, ARC Ctr Excellence Quantum Atom Opt, Hawthorn, Vic 3122, Australia.
[Ticknor, Christopher] Swinburne Univ Technol, Ctr Atom Opt & Ultrafast Spect, Hawthorn, Vic 3122, Australia.
[Ticknor, Christopher] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Ticknor, C (reprint author), Swinburne Univ Technol, ARC Ctr Excellence Quantum Atom Opt, Hawthorn, Vic 3122, Australia.
RI Ticknor, Christopher/B-8651-2014
FU Australian Research Council; NSF through ITAMP at Harvard University;
Smithsonian Astrophysical Observatory
FX The author gratefully acknowledges support from the Australian Research
Council and partial support from NSF through ITAMP at Harvard University
and Smithsonian Astrophysical Observatory. The author thanks H. Hu and
X.-J. Li for incredibly enlightening discussions.
NR 26
TC 25
Z9 25
U1 1
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD NOV
PY 2009
VL 80
IS 5
AR 052702
DI 10.1103/PhysRevA.80.052702
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 526RH
UT WOS:000272310000083
ER
PT J
AU Tikhonenkov, I
Vardi, A
AF Tikhonenkov, I.
Vardi, A.
TI Atom-molecule dephasing in an SU(1,1) interferometer based on the
stimulated dissociation of a molecular Bose-Einstein condensate
SO PHYSICAL REVIEW A
LA English
DT Article
DE atom optics; atom-molecule collisions; Bose-Einstein condensation; SU(2)
theory
ID JOSEPHSON-JUNCTION; SUPERCHEMISTRY; PHASE
AB We propose to implement a sub-shot-noise matter-wave interferometer via the stimulated dissociation of a molecular Bose-Einstein condensate and study the collisional loss of atom-molecule coherence during its phase-acquisition time. The obtained n-atom states are two-atom [SU(1,1)] coherent states with number variance Delta n proportional to n compared to Delta n proportional to n for the spin [SU(2)] coherent states formed by coherent splitting of an atomic condensate. Consequently, the Lorentzian atom-molecule phase diffusion is faster than the Gaussian phase diffusion between separated atomic condensates by a n factor.
C1 [Tikhonenkov, I.; Vardi, A.] Ben Gurion Univ Negev, Dept Chem, IL-84105 Beer Sheva, Israel.
[Vardi, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Tikhonenkov, I (reprint author), Ben Gurion Univ Negev, Dept Chem, POB 653, IL-84105 Beer Sheva, Israel.
RI Vardi, Amichay/D-8189-2011
OI Vardi, Amichay/0000-0002-8992-2129
FU National Science Foundation through a grant for the Institute for
Theoretical Atomic, Molecular, and Optical Physics at Harvard
University; Israel Science Foundation [582/07]; United States-Israel
Binational Science Foundation (BSF) [2008141]
FX This work was supported by the National Science Foundation through a
grant for the Institute for Theoretical Atomic, Molecular, and Optical
Physics at Harvard University and Smithsonian Astrophysical Observatory,
by the Israel Science Foundation (Grant No. 582/07), and by the United
States-Israel Binational Science Foundation (BSF) (Grant No. 2008141)
NR 32
TC 6
Z9 6
U1 0
U2 5
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD NOV
PY 2009
VL 80
IS 5
AR 051604
DI 10.1103/PhysRevA.80.051604
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 526RH
UT WOS:000272310000016
ER
PT J
AU Zhang, WX
Cappellaro, P
Antler, N
Pepper, B
Cory, DG
Dobrovitski, VV
Ramanathan, C
Viola, L
AF Zhang, Wenxian
Cappellaro, Paola
Antler, Natania
Pepper, Brian
Cory, David G.
Dobrovitski, Viatcheslav V.
Ramanathan, Chandrasekhar
Viola, Lorenza
TI NMR multiple quantum coherences in quasi-one-dimensional spin systems:
Comparison with ideal spin-chain dynamics
SO PHYSICAL REVIEW A
LA English
DT Article
DE calcium compounds; nuclear magnetic resonance; numerical analysis;
quantum wires; spin dynamics; spin Hamiltonians; spin systems
ID NUCLEAR-MAGNETIC-RESONANCE; LINE-SHAPE; SOLIDS; DIAMOND; TEMPERATURE;
TRANSITIONS; EXCITATION; QUBITS
AB The F-19 spins in a crystal of fluorapatite have often been used to experimentally approximate a one-dimensional spin system. Under suitable multipulse control, the nuclear-spin dynamics may be modeled to first approximation by a double-quantum one-dimensional Hamiltonian, which is analytically solvable for nearest-neighbor couplings. Here, we use solid-state nuclear magnetic resonance techniques to investigate the multiple quantum coherence dynamics of fluorapatite, with an emphasis on understanding the region of validity for such a simplified picture. Using experimental, numerical, and analytical methods, we explore the effects of long-range intrachain couplings, cross-chain couplings, as well as couplings to a spin environment, all of which tend to damp the oscillations of the multiple quantum coherence signal at sufficiently long times. Our analysis characterizes the extent to which fluorapatite can faithfully simulate a one-dimensional quantum wire.
C1 [Zhang, Wenxian; Viola, Lorenza] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Zhang, Wenxian] Fudan Univ, Dep Opt Sci & Engn, Shanghai 200433, Peoples R China.
[Cappellaro, Paola] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Cappellaro, Paola; Cory, David G.; Ramanathan, Chandrasekhar] MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA.
[Antler, Natania; Pepper, Brian] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Dobrovitski, Viatcheslav V.] Iowa State Univ, Ames Lab, US DOE, Ames, IA 50011 USA.
RP Zhang, WX (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
EM lorenza.viola@dartmouth.edu
RI Zhang, Wenxian/A-4274-2010; Cappellaro, Paola/B-1413-2010; Ramanathan,
Chandrasekhar/C-5207-2008
OI Cappellaro, Paola/0000-0003-3207-594X; Ramanathan,
Chandrasekhar/0000-0002-7457-3608
NR 58
TC 21
Z9 21
U1 0
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD NOV
PY 2009
VL 80
IS 5
AR 052323
DI 10.1103/PhysRevA.80.052323
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 526RH
UT WOS:000272310000058
ER
PT J
AU Cernusak, LA
Winter, K
Turner, BL
AF Cernusak, Lucas A.
Winter, Klaus
Turner, Benjamin L.
TI Plant delta N-15 Correlates with the Transpiration Efficiency of
Nitrogen Acquisition in Tropical Trees
SO PLANT PHYSIOLOGY
LA English
DT Article
ID N-15 NATURAL-ABUNDANCE; ISOTOPE COMPOSITION; NITRATE ASSIMILATION;
FOLIAR DELTA-N-15; SPINACH LEAVES; USE STRATEGIES; AMMONIUM;
FRACTIONATION; WATER; DELTA-C-13
AB Based upon considerations of a theoretical model of N-15/N-14 fractionation during steady-state nitrate uptake from soil, we hypothesized that, for plants grown in a common soil environment, whole-plant delta N-15 (delta(P)) should vary as a function of the transpiration efficiency of nitrogen acquisition (F-N/nu) and the difference between delta(P) and root delta N-15 (delta(P) - delta(R)). We tested these hypotheses with measurements of several tropical tree and liana species. Consistent with theoretical expectations, both F-N/v and delta(P) - delta(R) were significant sources of variation in delta(P), and the relationship between delta(P) and F-N/v differed between non-N-2-fixing and N-2-fixing species. We interpret the correlation between delta(P) and F-N/nu as resulting from variation in mineral nitrogen efflux-to-influx ratios across plasma membranes of root cells. These results provide a simple explanation of variation in delta N-15 of terrestrial plants and have implications for understanding nitrogen cycling in ecosystems.
C1 [Cernusak, Lucas A.; Winter, Klaus; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Cernusak, LA (reprint author), Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia.
EM lucas.cernusak@cdu.edu.au
RI Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011
OI Turner, Benjamin/0000-0002-6585-0722; Cernusak,
Lucas/0000-0002-7575-5526
FU Smithsonian Tropical Research Institute; Australian Research Council
FX This work was supported by a Tupper Postdoctoral Fellowship from the
Smithsonian Tropical Research Institute and by an Australian
Postdoctoral Fellowship from the Australian Research Council, both to L.
A. C.
NR 65
TC 23
Z9 23
U1 0
U2 24
PU AMER SOC PLANT BIOLOGISTS
PI ROCKVILLE
PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA
SN 0032-0889
J9 PLANT PHYSIOL
JI Plant Physiol.
PD NOV
PY 2009
VL 151
IS 3
BP 1667
EP 1676
DI 10.1104/pp.109.145870
PG 10
WC Plant Sciences
SC Plant Sciences
GA 514XQ
UT WOS:000271430500061
PM 19726571
ER
PT J
AU Steiner, JF
Narayan, R
McClintock, JE
Ebisawa, K
AF Steiner, James F.
Narayan, Ramesh
McClintock, Jeffrey E.
Ebisawa, Ken
TI A Simple Comptonization Model
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID BLACK-HOLE SPIN; X-RAY BINARIES; HIGH-ENERGY SPECTRA; CYGNUS X-1; LMC
X-3; SPECTROSCOPY; ACCRETION; RADIATION; OUTBURST; PLASMA
AB We present an empirical model of Comptonization for fitting the spectra of X-ray binaries. This model, named SIMPL, has been developed as a package implemented in XSPEC. With only two free parameters, SIMPL is competitive as the simplest model of Compton scattering. Unlike the pervasive standard power-law model, SIMPL incorporates the basic features of Compton scattering of soft photons by energetic coronal electrons. Using a simulated spectrum, we demonstrate that SIMPL closely matches the behavior of physical Comptonization models that consider the effects of optical depth, coronal electron temperature, and geometry. We present fits to RXTE spectra of the black hole transient H1743-322 and a BeppoSAX spectrum of LMC X-3 using both SIMPL and the standard power-law model. A comparison of the results shows that SIMPL gives equally good fits, while eliminating the troublesome divergence of the standard power-law model at low energies. SIMPL is completely flexible and can be used self-consistently with any seed spectrum of photons. We show an example of how SIMPL-unlike the standard power law-teamed up with DISKBB (the standard model of disk accretion) provides a uniform disk normalization that is unaffected by moderate Comptonization.
C1 [Steiner, James F.; Narayan, Ramesh; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ebisawa, Ken] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jsteiner@cfa.harvard.edu
FU Smithsonian Institution Endowment Funds; NASA [NNX08AH32G, NNX08AJ55G];
NSF [AST0805832]
FX The authors would like to thank George Rybicki for discussions on the
physics of Comptonization as well as Jifeng Liu, Lijun Gou, Rebecca
Shafee, and Ron Remillard for their input on SIMPL. J. F. S. thanks Joey
Neilsen for enthusiastic discussions as well as comments on the
manuscript, Ryan Hickox for ideas which improved this article, Irwin
Shapiro for his suggestions on the manuscript, and Keith Arnaud for
helping implement SIMPL in XSPEC. The authors thank Tim Oosterbroek for
his indefatigable assistance with the BeppoSAX reduction software. J. F.
S. was supported by the Smithsonian Institution Endowment Funds and R.
N. acknowledges support from NASA grant NNX08AH32G and NSF grant
AST0805832. J. E. M. acknowledges support from NASA grant NNX08AJ55G.
NR 41
TC 93
Z9 93
U1 1
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD NOV
PY 2009
VL 121
IS 885
BP 1279
EP 1290
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 511UB
UT WOS:000271193700012
ER
PT J
AU Woodman, N
Athfield, NB
AF Woodman, Neal
Athfield, Nancy Beavan
TI Post-Clovis survival of American Mastodon in the southern Great Lakes
Region of North America
SO QUATERNARY RESEARCH
LA English
DT Article
DE Accelerator mass spectrometer; Extinction; Indiana; Mammal; Paleoindian;
Radiocarbon
ID PLEISTOCENE MAMMALIAN EXTINCTIONS; CALIBRATION PROGRAM; AGE CALIBRATION;
LATE QUATERNARY; BONE-COLLAGEN; C-14 DATA; INDIANA; PALEOECOLOGY;
MAMMOTH; RECORD
AB The end of the Pleistocene in North America was marked by a wave of extinctions of large mammals, with the last known appearances of many species falling between ca 11,000-10,000 (14)C yr BP Temporally, this period overlaps with the Clovis Paleoindian cultural complex (11,190-10,530 (14)C yr BP) and with sudden climatic changes that define the beginning of the Younger Dryas chronozone (ca 11,000-10,000 (14)C yr BP), both of which have been considered as potential proximal causes of this extinction event Radiocarbon dating of enamel and filtered bone collagen from an extinct American Mastodon (Mammut americanum) from northern Indiana, USA, by accelerator mass spectrometer yielded direct dates of 10,055 +/- 40 (14)C yr BP and 10,032 +/- 40 (14)C yr BP indicating that the animal survived beyond the Clovis time period and into the late Younger Dryas Although the late survival of this species in mid-continental North America does nor remove either humans or climatic change as contributing causes for the late Pleistocene extinctions, neither Clovis hunters nor the climatic perturbations initiating the Younger Dryas chronozone were immediately responsible for driving mastodons to extinction. (C) 2009 University of Washington Published by Elsevier Inc All rights reserved.
C1 [Woodman, Neal] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, MRC 111, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Athfield, Nancy Beavan] GNS Sci, Natl Isotope Ctr, Lower Hutt, New Zealand.
RP Woodman, N (reprint author), Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, MRC 111, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM woodmann@si.edu
NR 52
TC 12
Z9 12
U1 2
U2 17
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0033-5894
J9 QUATERNARY RES
JI Quat. Res.
PD NOV
PY 2009
VL 72
IS 3
BP 359
EP 363
DI 10.1016/j.yqres.2009.06.009
PG 5
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 512MQ
UT WOS:000271254000006
ER
PT J
AU Craven, D
Hall, J
Verjans, JM
AF Craven, Dylan
Hall, Jefferson
Verjans, Jean-Marc
TI Impacts of Herbicide Application and Mechanical Cleanings on Growth and
Mortality of Two Timber Species in Saccharum spontaneum Grasslands of
the Panama Canal Watershed
SO RESTORATION ECOLOGY
LA English
DT Article
DE invasive grass species; Panama; reforestation; Tectona grandis;
Terminalia amazonia
ID COSTA-RICA; IMPERATA-CYLINDRICA; FOREST PLANTATIONS; ABANDONED PASTURE;
PHOTOSYNTHETIC RESPONSES; DRY FOREST; RESTORATION; REGENERATION;
PERFORMANCE; SEEDLINGS
AB Reforestation has been suggested as a strategy to control Saccharum spontaneum, an invasive grass that impedes regeneration in disturbed areas of the Panama Canal Watershed (PCW). In this study, the effects of different intensities of herbicide application and mechanical cleanings on the growth and mortality of Terminalia amazonia and Tectona grandis saplings were evaluated in S. spontaneum grasslands within the PCW. Both species exhibited greater height, basal diameter, wood volume index, wider crown diameters, deeper live crowns, and lower mortality with increasing intensity of mechanical cleanings and herbicide application. Height and competition of S. spontaneum correlated negatively with intensity of mechanical cleanings and herbicide application. Grass control costs did not differ between tree species but did increase significantly with intensity of mechanical cleanings and herbicide application. We recommend fire suppression, annual herbicide application, and at least four mechanical cleanings per year in Tec. grandis plantations during the first 3 years of plantation establishment. Given the slower initial growth and mortality patterns of Ter. amazonia, aggressive grass control treatments should be continued until individuals are sufficiently large to effectively shade S. spontaneum. Results from this study suggest that reforestation with commercial timber species can rapidly establish and control S. spontaneum growth in the PCW. Reforestation of areas already invaded or at risk of being invaded by S. spontaneum appears to be a viable strategy to reduce its abundance and subsequent negative ecological effects in the PCW.
C1 [Craven, Dylan; Hall, Jefferson] Smithsonian Trop Res Inst, Native Species Reforestat Project PRORENA, Appl Ecol Program, Ctr Trop Forest Sci, Balboa, Ancon, Panama.
[Verjans, Jean-Marc] Ecoforest SA, Balboa, Ancon, Panama.
RP Craven, D (reprint author), Smithsonian Trop Res Inst, Native Species Reforestat Project PRORENA, Appl Ecol Program, Ctr Trop Forest Sci, Ave Roosevelt 401, Balboa, Ancon, Panama.
EM dylan.craven@yale.edu
RI Craven, Dylan/K-2717-2012
OI Craven, Dylan/0000-0003-3940-833X
FU Native Species Reforestation Project (PRORENA) and Eco-Forest; Center of
Tropical Forest Science at the Smithsonian Institute of Tropical
Research Investigation and Yale University's School of Forestry and
Environmental Studies
FX This project was part of a collaborative research program between the
Native Species Reforestation Project (PRORENA) and Eco-Forest S.A.
PRORENA is a joint research initiative between the Applied Ecology
Program of the Center of Tropical Forest Science at the Smithsonian
Institute of Tropical Research Investigation and Yale University's
School of Forestry and Environmental Studies. The authors would like to
thank the following people for their valuable contributions: M. Wishnie,
N. Cedeno, E. Marisical, J. Deago, L. Irland, PRORENA staff, Eco-Forest
S.A. staff, and two anonymous reviewers.
NR 57
TC 18
Z9 19
U1 1
U2 16
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1061-2971
J9 RESTOR ECOL
JI Restor. Ecol.
PD NOV
PY 2009
VL 17
IS 6
BP 751
EP 761
DI 10.1111/j.1526-100X.2008.00408.x
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 524GL
UT WOS:000272131700001
ER
PT J
AU Lin, J
AF Lin Jun
TI Studies of solar flares and CMEs related to the space solar missions in
the future
SO SCIENCE IN CHINA SERIES G-PHYSICS MECHANICS & ASTRONOMY
LA English
DT Article; Proceedings Paper
CT Solar Workshop on Solar Magnetism, Corona and Space Weather - Chinese
Space Solar Telescope Science
CY JUL 28-AUG 01, 2008
CL Jiuquan, PEOPLES R CHINA
DE solar eruptions; magnetic field; energy conversion; magnetic
reconnection; current sheet
ID CORONAL MASS EJECTIONS; X-RAY FLARES; EMERGING FLUX; CURRENT SHEETS;
MAGNETIC RECONNECTION; ACTIVE REGIONS; RADIO OBSERVATIONS; EIT WAVES;
H-ALPHA; ERUPTIONS
AB Solar eruptions and the related processes involve magnetic fields and plasma flows of various scales in both time and space. These processes include the convective motions of the mass and magnetic field in the photosphere, evolutions of magnetic fields in both the chromosphere and the corona prior to and during the disruption of magnetic fields in response to the photospheric motions. These evolutions constitute a whole process of transporting the magnetic energy and the helicity from the photosphere to the corona, and then to interplanetary space. The present work, on the basis of a solar eruption model, discusses these processes, and the related questions, unanswerable at present, but could be the scientific objectives of the space solar missions in the future.
C1 [Lin Jun] Chinese Acad Sci, Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Peoples R China.
[Lin Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lin, J (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Peoples R China.
EM jlin@ynao.ac.cn
RI LIN, JUN/B-9890-2017
NR 97
TC 3
Z9 4
U1 0
U2 1
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1672-1799
J9 SCI CHINA SER G
JI Sci. China Ser. G-Phys. Mech. Astron.
PD NOV
PY 2009
VL 52
IS 11
SI SI
BP 1646
EP 1654
DI 10.1007/s11433-009-0242-7
PG 9
WC Physics, Multidisciplinary
SC Physics
GA 518UB
UT WOS:000271718600003
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI FDR's Stamps
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD NOV
PY 2009
VL 40
IS 8
BP 22
EP 22
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 509XB
UT WOS:000271051500010
ER
PT J
AU Turner, BL
Romero, TE
AF Turner, Benjamin L.
Romero, Tania E.
TI Short-Term Changes in Extractable Inorganic Nutrients during Storage of
Tropical Rain Forest Soils
SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL
LA English
DT Article
ID AIR-DRIED SOILS; PHOSPHORUS SOLUBILIZATION; PASTURE SOILS; SAMPLES;
PHOSPHATE; DYNAMICS; SORPTION; RESIN; ADSORPTION; PATTERNS
AB The nutrient status of tropical forests is commonly assessed by measuring inorganic nutrients extracted from soil, yet samples from remote research sites may be stored for prolonged periods of time before analysis. We assessed the influence of soil storage conditions on extractable nutrients in three lowland tropical forests soils from the Republic of Panama. The soils spanned a strong rainfall gradient and contained contrasting chemical and physical properties. Storage treatments were: (i) room temperature (22 degrees C in the dark), (ii) refrigerated (4 degrees C in the dark), (iii) air dried (10 d at 22 degrees C and 55% humidity), and (iv) frozen (-35 degrees C). Ammonium and NO(3) were extremely unstable and concentrations changed considerably within hours of sampling. Phosphate extracted by anion-exchange membranes also changed rapidly following sampling, although cations (Ca, K, and Mg) extracted in Mehlich-3 solution were less influenced by storage. Soil pH declined slowly in A samples during field-moist storage (4 and 22 degrees C). Freezing and air drying generally caused significant changes in extractable nutrients, although the effects varied among soils and nutrients. We therefore conclude that inorganic nutrients should be extracted from tropical forest soils within 24 h of sampling, and preferably on the day of sampling for N fractions, to ensure that values represent field conditions. Where this is not possible, rapid air drying or storage of field-moist samples may be acceptable for some measurements (e.g., PO(4), cations, pH), but are unlikely to provide realistic measurements of inorganic N.
C1 [Turner, Benjamin L.; Romero, Tania E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM TurnerBL@si.edu
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
NR 40
TC 40
Z9 40
U1 1
U2 23
PU SOIL SCI SOC AMER
PI MADISON
PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA
SN 0361-5995
J9 SOIL SCI SOC AM J
JI Soil Sci. Soc. Am. J.
PD NOV-DEC
PY 2009
VL 73
IS 6
BP 1972
EP 1979
DI 10.2136/sssaj2008.0407
PG 8
WC Soil Science
SC Agriculture
GA 519GJ
UT WOS:000271752700026
ER
PT J
AU Wurdack, KJ
Dorr, LJ
AF Wurdack, Kenneth J.
Dorr, Laurence J.
TI The South American genera of Hemerocallidaceae (Eccremis and Pasithea):
two introductions to the New World
SO TAXON
LA English
DT Article
DE Asparagales; biogeography; Eccremis; molecular phylogenetics; taxonomy
ID STYPANDRA-IMBRICATA; DNA-SEQUENCES; PHYLOGENETIC-RELATIONSHIPS;
EVOLUTIONARY SIGNIFICANCE; DIANELLA-REVOLUTA; FLOWERING PLANTS;
CHLOROPLAST DNA; FLESHY FRUITS; PLASTID RBCL; SENSU-LATO
AB Two unispecific genera. Eccremis and Pasithea, are the only representatives of Hemerocallidaceae (Asparagales) native to the Western Hemisphere. The affinities of the former genus have been recently questioned. Phylogenetic analyses of DNA sequence data (plastid atpB, ndhF, rbcL, trnL-F) spanning the Asparagales recover a monophyletic Hemerocallidaceae and strongly support the inclusion of Eccremis within that family. Eccremis is sister to Dianella and not closely associated with Pasithea, which indicates two introductions of Hemerocallidaceae to the New World. A taxonomic synopsis of Eccremis and Pasithea is presented and morphological character evolution and biogeography are discussed.
C1 [Wurdack, Kenneth J.; Dorr, Laurence J.] Natl Museum Nat Hist, Dept Bot, MRC 166, Smithsonian Inst, Washington, DC 20013 USA.
RP Wurdack, KJ (reprint author), Natl Museum Nat Hist, Dept Bot, MRC 166, Smithsonian Inst, POB 37012, Washington, DC 20013 USA.
EM wurdackk@si.edu
NR 77
TC 9
Z9 9
U1 1
U2 3
PU INT ASSOC PLANT TAXONOMY
PI VIENNA
PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA
SN 0040-0262
J9 TAXON
JI Taxon
PD NOV
PY 2009
VL 58
IS 4
BP 1122
EP 1132
PG 11
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 524HH
UT WOS:000272133900006
ER
PT J
AU Dorr, LJ
AF Dorr, Laurence J.
TI xChiranthomontodendron: the correct nothogeneric name for the artificial
hybrid Chiranthodendron x Fremontodendron (Malvaceae: Malvoideae)
SO TAXON
LA English
DT Editorial Material
DE Chiranthodendron; xChiranthofremontia; xChiranthomontodendron;
Fremontodendron; Malvaceae; nothogenus
AB The nothogeneric name xChiranthomontodendron is proposed to accommodate an artificial hybrid between species of Chiranthodendron and Fremontodendron, and the nothospecies xChiranthomontodendron lenzii is described from cultivated material.
C1 Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, Washington, DC 20013 USA.
RP Dorr, LJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, POB 37012, Washington, DC 20013 USA.
EM dorrl@si.edu
NR 4
TC 0
Z9 0
U1 0
U2 0
PU INT ASSOC PLANT TAXONOMY-IAPT
PI BRATISLAVA
PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23
BRATISLAVA, SLOVAKIA
SN 0040-0262
EI 1996-8175
J9 TAXON
JI Taxon
PD NOV
PY 2009
VL 58
IS 4
BP 1357
EP 1358
PG 2
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 524HH
UT WOS:000272133900023
ER
PT J
AU Tanvir, NR
Fox, DB
Levan, AJ
Berger, E
Wiersema, K
Fynbo, JPU
Cucchiara, A
Kruhler, T
Gehrels, N
Bloom, JS
Greiner, J
Evans, PA
Rol, E
Olivares, F
Hjorth, J
Jakobsson, P
Farihi, J
Willingale, R
Starling, RLC
Cenko, SB
Perley, D
Maund, JR
Duke, J
Wijers, RAMJ
Adamson, AJ
Allan, A
Bremer, MN
Burrows, DN
Castro-Tirado, AJ
Cavanagh, B
Postigo, AD
Dopita, MA
Fatkhullin, TA
Fruchter, AS
Foley, RJ
Gorosabel, J
Kennea, J
Kerr, T
Klose, S
Krimm, HA
Komarova, VN
Kulkarni, SR
Moskvitin, AS
Mundell, CG
Naylor, T
Page, K
Penprase, BE
Perri, M
Podsiadlowski, P
Roth, K
Rutledge, RE
Sakamoto, T
Schady, P
Schmidt, BP
Soderberg, AM
Sollerman, J
Stephens, AW
Stratta, G
Ukwatta, TN
Watson, D
Westra, E
Wold, T
Wolf, C
AF Tanvir, N. R.
Fox, D. B.
Levan, A. J.
Berger, E.
Wiersema, K.
Fynbo, J. P. U.
Cucchiara, A.
Kruehler, T.
Gehrels, N.
Bloom, J. S.
Greiner, J.
Evans, P. A.
Rol, E.
Olivares, F.
Hjorth, J.
Jakobsson, P.
Farihi, J.
Willingale, R.
Starling, R. L. C.
Cenko, S. B.
Perley, D.
Maund, J. R.
Duke, J.
Wijers, R. A. M. J.
Adamson, A. J.
Allan, A.
Bremer, M. N.
Burrows, D. N.
Castro-Tirado, A. J.
Cavanagh, B.
de Ugarte Postigo, A.
Dopita, M. A.
Fatkhullin, T. A.
Fruchter, A. S.
Foley, R. J.
Gorosabel, J.
Kennea, J.
Kerr, T.
Klose, S.
Krimm, H. A.
Komarova, V. N.
Kulkarni, S. R.
Moskvitin, A. S.
Mundell, C. G.
Naylor, T.
Page, K.
Penprase, B. E.
Perri, M.
Podsiadlowski, P.
Roth, K.
Rutledge, R. E.
Sakamoto, T.
Schady, P.
Schmidt, B. P.
Soderberg, A. M.
Sollerman, J.
Stephens, A. W.
Stratta, G.
Ukwatta, T. N.
Watson, D.
Westra, E.
Wold, T.
Wolf, C.
TI A gamma-ray burst at a redshift of z approximate to 8.2
SO NATURE
LA English
DT Article
ID REIONIZATION; AFTERGLOW; SWIFT; EVOLUTION; FRACTION; UNIVERSE; GALAXY;
PROBE; GRBS
AB Long-duration gamma-ray bursts (GRBs) are thought to result from the explosions of certain massive stars(1), and some are bright enough that they should be observable out to redshifts of z > 20 using current technology(2-4). Hitherto, the highest redshift measured for any object was z = 6.96, for a Lyman-alpha emitting galaxy(5). Here we report that GRB 090423 lies at a redshift of z approximate to 8.2, implying that massive stars were being produced and dying as GRBs similar to 630 Myr after the Big Bang. The burst also pinpoints the location of its host galaxy.
C1 [Tanvir, N. R.; Wiersema, K.; Evans, P. A.; Farihi, J.; Willingale, R.; Starling, R. L. C.; Duke, J.; Page, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Fox, D. B.; Cucchiara, A.; Burrows, D. N.; Kennea, J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Berger, E.; Foley, R. J.; Soderberg, A. M.; Westra, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fynbo, J. P. U.; Hjorth, J.; Maund, J. R.; Sollerman, J.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Kruehler, T.; Greiner, J.; Olivares, F.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
[Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[Gehrels, N.; Krimm, H. A.; Sakamoto, T.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bloom, J. S.; Cenko, S. B.; Perley, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rol, E.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[Adamson, A. J.; Cavanagh, B.; Kerr, T.; Wold, T.] Joint Astron Ctr, Hilo, HI 96720 USA.
[Allan, A.; Naylor, T.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Castro-Tirado, A. J.; Gorosabel, J.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[de Ugarte Postigo, A.] European So Observ, Santiago 19, Chile.
[Dopita, M. A.; Schmidt, B. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Fatkhullin, T. A.; Komarova, V. N.; Moskvitin, A. S.] Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia.
[Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Krimm, H. A.; Sakamoto, T.] CRESST, Greenbelt, MD 20771 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Mundell, C. G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Penprase, B. E.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Perri, M.; Stratta, G.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Podsiadlowski, P.; Wolf, C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Roth, K.; Stephens, A. W.] Gemini Observ, Hilo, HI 96720 USA.
[Rutledge, R. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Schady, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Sollerman, J.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Ukwatta, T. N.] George Washington Univ, Washington, DC 20052 USA.
RP Tanvir, NR (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM nrt3@star.le.ac.uk
RI Jakobsson, Pall/L-9950-2015; Stratta, Maria Giuliana/L-3045-2016;
Gehrels, Neil/D-2971-2012; Fynbo, Johan/L-8496-2014; Hjorth,
Jens/M-5787-2014; Dopita, Michael/P-5413-2014; Naylor, Tim /A-9465-2015;
Watson, Darach/E-4521-2015
OI Jakobsson, Pall/0000-0002-9404-5650; Stratta, Maria
Giuliana/0000-0003-1055-7980; Wijers, Ralph/0000-0002-3101-1808; Fynbo,
Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Dopita,
Michael/0000-0003-0922-4986; Watson, Darach/0000-0002-4465-8264
FU Clay Fellowship
FX We thank Ph. Yock, B. Allen, P. Kubanek, M. Jelinek and S. Guziy for
their assistance with the BOOTES-3 YA telescope observations
(Supplementary Information). This work was partly 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 US National Science Foundation on behalf of the
Gemini partnership: the National Science Foundation (United States), the
Science and Technology Facilities Council (United Kingdom), the National
Research Council (Canada), CONICYT (Chile), the Australian Research
Council (Australia), the Ministerio da Ciencia e Tecnologia (Brazil) and
SECYT (Argentina). This work was also partly based on observations made
using ESO telescopes at the La Silla or Paranal observatories by G.
Carraro, L. Schmidtobreick, G. Marconi, J. Smoker, V. Ivanov, E. Mason
and M. Huertas-Company. The UKIRT is operated by the Joint Astronomy
Centre on behalf of the UK Science and Technology Facilities Council. R.
J. F. acknowledges a Clay Fellowship.
NR 27
TC 353
Z9 357
U1 4
U2 20
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD OCT 29
PY 2009
VL 461
IS 7268
BP 1254
EP 1257
DI 10.1038/nature08459
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 511TF
UT WOS:000271190800042
PM 19865165
ER
PT J
AU Kursar, TA
Dexter, KG
Lokvam, J
Pennington, RT
Richardson, JE
Weber, MG
Murakami, ET
Drake, C
McGregor, R
Coley, PD
AF Kursar, Thomas A.
Dexter, Kyle G.
Lokvam, John
Pennington, R. Toby
Richardson, James E.
Weber, Marjorie G.
Murakami, Eric T.
Drake, Camilla
McGregor, Ruth
Coley, Phyllis D.
TI The evolution of antiherbivore defenses and their contribution to
species coexistence in the tropical tree genus Inga
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE plant defenses; community assembly; phylogenetic signal; herbivory;
tropical diversity
ID RAIN-FOREST TREES; YOUNG LEAVES; CHLOROPLAST DNA; PLANT DEFENSE;
AMINO-ACIDS; UMBELLIFERA FABACEAE; PHYLOGENETIC SIGNAL; NONCODING
REGIONS; LEAF DEVELOPMENT; STRATEGIES
AB Plants and their herbivores constitute more than half of the organisms in tropical forests. Therefore, a better understanding of the evolution of plant defenses against their herbivores may be central for our understanding of tropical biodiversity. Here, we address the evolution of antiherbivore defenses and their possible contribution to coexistence in the Neotropical tree genus Inga (Fabaceae). Inga has > 300 species, has radiated recently, and is frequently one of the most diverse and abundant genera at a given site. For 37 species from Panama and Peru we characterized developmental, ant, and chemical defenses against herbivores. We found extensive variation in defenses, but little evidence of phylogenetic signal. Furthermore, in a multivariate analysis, developmental, ant, and chemical defenses varied independently (were orthogonal) and appear to have evolved independently of each other. Our results are consistent with strong selection for divergent defensive traits, presumably mediated by herbivores. In an analysis of community assembly, we found that Inga species co-occurring as neighbors are more different in antiherbivore defenses than random, suggesting that possessing a rare defense phenotype increases fitness. These results imply that interactions with herbivores may be an important axis of niche differentiation that permits the coexistence of many species of Inga within a single site. Interactions between plants and their herbivores likely play a key role in the generation and maintenance of the conspicuously high plant diversity in the tropics.
C1 [Kursar, Thomas A.; Lokvam, John; Weber, Marjorie G.; Murakami, Eric T.; Coley, Phyllis D.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Kursar, Thomas A.; Coley, Phyllis D.] Smithsonian Trop Res Inst, Balboa, Panama.
[Dexter, Kyle G.] Univ Toulouse 3, CNRS, UMR 5174, Lab Evolut & Diversite Biol, F-31062 Toulouse, France.
[Pennington, R. Toby; Richardson, James E.; Drake, Camilla; McGregor, Ruth] Royal Bot Garden, Edinburgh EH3 5LR, Midlothian, Scotland.
RP Kursar, TA (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
EM kursar@biology.utah.edu
RI Richardson, James-Edward/L-2768-2016
OI Richardson, James-Edward/0000-0001-9014-4865
FU National Science Foundation [DDIG-0608368, DEB-0234936, DEB-0640630];
Amazon Conservation Association; American Philosophical Society; Duke
University; Explorer's Club; Society for Systematic Biology; Sigma Xi;
Leverhulme Trust Study [RF/2/2006/0142]
FX We thank E. Leigh for stimulating discussions and O. Acevedo and B.
Jimenez for moral and logistical support at the Smithsonian Tropical
Research Institute; K. Rudolph, K. Bromberg, D. Dvorett, S. Ring, B.
Wolfe, and M.-J. Epps for field assistance in Panama; N. Pitman for
intellectual input and J. Saldana, C. Lazo, and F. Para for field work
in Peru; officials from Autoridad Nacional del Ambiente of Panama and
Instituto Nacional de Recursos Naturales of Peru for permission to
conduct field work; S. Lee and D. Grapov for assistance with the
chemical characterizations at the University of Utah; officials at the
Center for Tropical Forest Science of the Smithsonian Tropical Research
Institute for use of the data from the 50-ha plot
(http://ctfs.si.edu/datasets/bci); and M. Lavin, M. Lemes, M.
Hollingsworth, and A. Clark for phylogenetic research. K. G. D. was
supported by National Science Foundation Grant DDIG-0608368 and grants
from the Amazon Conservation Association, American Philosophical
Society, Duke University, Explorer's Club, Society for Systematic
Biology, and Sigma Xi. T. A. K. and P. D. C. were supported by National
Science Foundation Grants DEB-0234936 and DEB-0640630 and Research
Experience for Undergraduate supplements. R. T. P. was supported by
Leverhulme Trust Study Abroad Fellowship RF/2/2006/0142.
NR 59
TC 94
Z9 96
U1 8
U2 89
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD OCT 27
PY 2009
VL 106
IS 43
BP 18073
EP 18078
DI 10.1073/pnas.0904786106
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 512DB
UT WOS:000271222500009
PM 19805183
ER
PT J
AU Burns, JM
Janzen, DH
Hallwachs, W
Hajibabaei, M
Hebert, PDN
AF Burns, John M.
Janzen, Daniel H.
Hallwachs, Winnie
Hajibabaei, Mehrdad
Hebert, Paul D. N.
TI GENITALIA, DNA BARCODES, AND LIFE HISTORIES SYNONYMIZE TELLES WITH
THRACIDES-A GENUS IN WHICH TELLES ARCALAUS LOOKS OUT OF PLACE
(HESPERIIDAE: HESPERIINAE)
SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY
LA English
DT Article
DE morphospecies; secondary sex character; panneotropic; Zingiberales;
Cyclanthaceae; "Telles" pyrex Evans incertae sedis
AB Independent characters-genitalia (male and female), DNA barcodes, and larval foodplants-show that Telles arcalaus (Stoll), despite its exceedingly distinctive facies and small size, belongs in the genus Thracides, where it relates closely to Thracides phidon (Cramer). Because phidon and arcalaus are the type species of their respective genera and Thracides is the older name, Telles is a synonym of Thracides. Because the only other species in Telles, T. pyrex Evans, is not a species of Thracides, it is incertae sedis. Either in Trinidad or in Para. Brazil, as in Area de Conservacion Guanacaste (ACG), Costa Rica, caterpillars of Thracides phidon and Thracides arcalaus, new combination, eat plants in the genera Heliconia and Musa (Zingriberales), whereas members of the Thracides uanea species complex eat Cyclanthus and Asplundia (Cyclanthaceae). Taxa of the mostly South American nanea species complex include Thracides nida Evans, new status and, in ACG T. chiricana Rober, new status. For now, owing to the numbers of cryptic species recently discovered within supposedly well-known species of neotropic hesperiids, the taxa treated here are viewed as morphospecies. DNA barcodes, which have proved so useful in distinguishing among cryptic species, are noteworthy ill this study for supporting the union in a single genus of ostensibly unrelated species.
C1 [Burns, John M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
[Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA.
[Hajibabaei, Mehrdad; Hebert, Paul D. N.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
RP Burns, JM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 127,Room E-515, Washington, DC 20013 USA.
EM burnsj@si.edu; djanzen@sas.upenn.edu; whallwac@sas.upenn.edu;
mhajibab@uoguelph.ca; phebert@uoguelph.ca
RI Hebert, Paul/C-4161-2013
OI Hebert, Paul/0000-0002-3081-6700
FU National Museum of Natural History Small Grunts Program; National
Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730,
0515699]; Gordon and Betty Moore Foundation; Genome Canada through the
Ontario Genomics Institute
FX We thank Sarah Burns for divers assistance, Donald Harvey for dissecting
genitalia, Young Sohn for figuring genitalia, Karie Darrow for
photographing adults and assembling plates, Olaf Mielke for photos of
holotypes and the loan of critical specimens, Tanya Dapkey for plucking
and shipping legs for DNA barcoding, parataxonomists for finding and
rearing caterpillars and adults, ACG: for conserving the ecosystems in
which they live, Sujeevan Ratnasingham for facilitating analysis of the
DNA sequence data, and Stephanie Kirk for aid with lab work. Support for
this study came from the National Museum of Natural History Small Grunts
Program (J.M.B..); from National Science Foundation grants BSR 9024770
and DEB 9306296, 9400829, 9705072, 0072730, and 0515699 (D.H.J.); and
from grants from the Gordon and Betty Moore Foundation and Genome Canada
through the Ontario Genomics Institute (P.D.N.H.).
NR 15
TC 7
Z9 9
U1 0
U2 1
PU LEPIDOPTERISTS SOC
PI LOS ANGELES
PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA
SN 0024-0966
J9 J LEPID SOC
JI J. Lepid. Soc.
PD OCT 22
PY 2009
VL 63
IS 3
BP 141
EP 153
PG 13
WC Entomology
SC Entomology
GA 512IW
UT WOS:000271242400003
ER
PT J
AU O'Dea, A
Jackson, J
AF O'Dea, Aaron
Jackson, Jeremy
TI Environmental change drove macroevolution in cupuladriid bryozoans
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE faunal turnover; life-history evolution; extinction; Isthmus of Panama
ID NEOGENE CUPULADRIIDAE; TROPICAL AMERICA; FAUNAL TURNOVER; OPPOSITE
SIDES; PANAMA; ISTHMUS; EXTINCTION; ECOLOGY; HISTORY; EVOLUTION
AB Most macroevolutionary events are correlated with changes in the environment, but more rigorous evidence of cause and effect has been elusive. We compiled a 10 Myr record of origination and extinction, changes in mode of reproduction, morphologies and abundances of cupuladriid bryozoan species, spanning the time when primary productivity collapsed in the southwestern Caribbean as the Isthmus of Panama closed. The dominant mode of reproduction shifted dramatically from clonal to aclonal, due in part to a pulse of origination followed by extinction that was strongly selective in favour of aclonal species. Modern-day studies predict reduced clonality in increasingly oligotrophic conditions, thereby providing a mechanistic explanation supporting the hypothesis that the collapse in primary productivity was the cause of turnover. However, whereas originations were synchronous with changing environments, extinctions lagged 1-2 Myr. Extinct species failed to become more robust and reduce their rate of cloning when the new environmental conditions arose, and subsequently saw progressive reductions in abundance towards their delayed demise. Environmental change is therefore established as the root cause of macroevolutionary turnover despite the lag between origination and extinction.
C1 [O'Dea, Aaron; Jackson, Jeremy] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Panama City, Panama.
[O'Dea, Aaron] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada.
[Jackson, Jeremy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Apartado 0843-03092, Panama City, Panama.
EM odeaa@si.edu
RI O'Dea, Aaron/D-4114-2011
FU National Science Foundation [EAR03-45471]; Smithsonian Marine Science
Network; Smithsonian Tropical Research Institutes' Tupper Fellowship;
Scholarly Studies programmes; SENACYT; National Geographic Society
Exploration
FX Felix Rodriguez, Brigida DeGracia and Yadixa DelValle identified,
counted and measured most of the cupuladriids. Anthony Coates, Helena
Fortunato, Amalia Herrera and many more helped collect, process and
analyse material. Egbert Leigh, Beth Okamura, Walton Green and Katie
Cramer made useful comments to the manuscript. The Panamanian Recursos
Minerales kindly gave permission to collect material. Funding was
provided by the National Science Foundation (EAR03-45471), the
Smithsonian Marine Science Network, the Smithsonian Tropical Research
Institutes' Tupper Fellowship and Scholarly Studies programmes, SENACYT
and the National Geographic Society Exploration Grants.
NR 34
TC 25
Z9 26
U1 0
U2 4
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P R SOC B
JI Proc. R. Soc. B-Biol. Sci.
PD OCT 22
PY 2009
VL 276
IS 1673
BP 3629
EP 3634
DI 10.1098/rspb.2009.0844
PG 6
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 498VF
UT WOS:000270172200008
PM 19640882
ER
PT J
AU Calvelo, DE
Vrtilek, SD
Steeghs, D
Torres, MAP
Neilsen, J
Filippenko, AV
Hernandez, JIG
AF Calvelo, D. E.
Vrtilek, S. D.
Steeghs, D.
Torres, M. A. P.
Neilsen, J.
Filippenko, A. V.
Hernandez, J. I. Gonzalez
TI Doppler and modulation tomography of XTE J1118+480 in quiescence
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; binaries: close; stars: individual: XTE
J1118+480
ID X-RAY TRANSIENT; BLACK-HOLE; ACCRETION DISC; GALACTIC HALO;
XTE-J1118+480; OUTBURST; SPECTROSCOPY; SUPERHUMPS; A0620-00; BINARY
AB We present Doppler and modulation tomography of the X-ray nova XTE J1118+480 with data obtained during quiescence using the 10-m Keck II telescope. The hotspot where the gas stream hits the accretion disc is seen in H alpha, H beta, He i lambda 5876 and Ca ii lambda 8662, thus verifying the presence of continued mass transfer within the system. The disc is clearly seen in H alpha and Ca ii lambda 8662. We image the mass-donor star in narrow absorption lines of Na i lambda lambda 5890, 5896, 8183, 8195 and Ca ii lambda 8662, implying an origin from the secondary itself rather than the interstellar medium. We also detect deviations in the centroid of the double peak of H alpha akin to those found by Zurita et al. suggesting disc eccentricity.
C1 [Calvelo, D. E.; Vrtilek, S. D.; Steeghs, D.; Torres, M. A. P.; Neilsen, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Calvelo, D. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Neilsen, J.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hernandez, J. I. Gonzalez] GEPI, Observ Paris Meudon, F-92195 Meudon, France.
RP Calvelo, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM d.e.calvelo@soton.ac.uk
RI Steeghs, Danny/C-5468-2009
OI Steeghs, Danny/0000-0003-0771-4746
FU W. M. Keck Foundation; NSF [AST-0507637, AST-0607485]; European
Commission [MEXT-CT-2004-014265]
FX 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 thank the Keck staff, as well as Ryan Chornock,
for their assistance with the observations. The ASM data are provided by
the ASM/RXTE teams at MIT and at the RXTE SOF and GOF at NASA's GSFC. We
acknowledge use of the MOLLY, DOPPLER and TRAILER software developed by
Tom Marsh, MODMAP developed by Danny Steeghs and the NIST Atomic Spectra
Data base. This work was supported by NSF grants AST-0507637 to SDV and
AST-0607485 to AVF. JIGH acknowledges support from European Commission
contract MEXT-CT-2004-014265 (CIFIST).
NR 32
TC 15
Z9 15
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2009
VL 399
IS 2
BP 539
EP 549
DI 10.1111/j.1365-2966.2009.15304.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 505AW
UT WOS:000270661300003
ER
PT J
AU Simha, V
Weinberg, DH
Dave, R
Gnedin, OY
Katz, N
Keres, D
AF Simha, Vimal
Weinberg, David H.
Dave, Romeel
Gnedin, Oleg Y.
Katz, Neal
Keres, Dusan
TI The growth of central and satellite galaxies in cosmological smoothed
particle hydrodynamics simulations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: formation
ID HALO OCCUPATION DISTRIBUTION; DIGITAL-SKY-SURVEY; COLD DARK-MATTER;
LUMINOSITY DEPENDENCE; SPH SIMULATIONS; REDSHIFT SURVEY; GAS; CLUSTERS;
Z-SIMILAR-TO-1; EVOLUTION
AB We examine the accretion and merger histories of central and satellite galaxies in a smoothed particle hydrodynamics (SPH) cosmological simulation that resolves galaxies down to 7 x 109 M(circle dot). Most friends-of-friends haloes in the simulation have a distinct central galaxy, typically 2-5 times more massive than the most massive satellite. As expected, satellites have systematically higher assembly redshifts than central galaxies of the same baryonic mass, and satellites in more massive haloes form earlier. However, contrary to the simplest expectations, satellite galaxies continue to accrete gas and convert it to stars; the gas accretion declines steadily over a period of 0.5-1 Gyr after the satellite halo merges with a larger parent halo. Satellites in a cluster mass halo eventually begin to lose baryonic mass. Typically, satellites in our simulation are 0.1-0.2 mag bluer than in models that assume no gas accretion on to satellites after a halo merger. Since z = 1, 27 per cent of central galaxies (above 3 x 1010 M(circle dot)) and 22 per cent of present-day satellite galaxies have merged with a smaller system above a 1:4 mass ratio; about half of the satellite mergers occurred after the galaxy became a satellite and half before. In effect, satellite galaxies can remain 'central' objects of halo substructures, with continuing accretion and mergers, making the transition in assembly histories and physical properties a gradual one. Implementing such a gradual transformation in semi-analytic models would improve their agreement with observed colour distributions of satellite galaxies in groups and with the observed colour dependence of galaxy clustering.
C1 [Simha, Vimal; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Simha, Vimal; Weinberg, David H.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Dave, Romeel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Gnedin, Oleg Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Katz, Neal] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Simha, V (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
EM vsimha@astronomy.ohio-state.edu; dhw@astronomy.ohio-state.edu;
rad@as.arizona.edu; ognedin@umich.edu; nsk@kaka.phast.umass.edu;
dkeres@cfa.harvard.edu
OI Gnedin, Oleg/0000-0001-9852-9954
FU NASA [NAG5-13308, NNG04GK68G]; Ohio State University Graduate Fellowship
FX We thank Mark Fardal and Ari Maller for useful discussions and technical
assistance, Charlie Conroy for providing a stellar population synthesis
package, Ralf Kotulla for assistance with the galev code and Roberto
Assef for useful discussions. This work was supported by NASA Grants
NAG5-13308 and NNG04GK68G and by an Ohio State University Graduate
Fellowship.
NR 61
TC 34
Z9 34
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2009
VL 399
IS 2
BP 650
EP 662
DI 10.1111/j.1365-2966.2009.15341.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 505AW
UT WOS:000270661300012
ER
PT J
AU Jones, DH
Read, MA
Saunders, W
Colless, M
Jarrett, T
Parker, QA
Fairall, AP
Mauch, T
Sadler, EM
Watson, FG
Burton, D
Campbell, LA
Cass, P
Croom, SM
Dawe, J
Fiegert, K
Frankcombe, L
Hartley, M
Huchra, J
James, D
Kirby, E
Lahav, O
Lucey, J
Mamon, GA
Moore, L
Peterson, BA
Prior, S
Proust, D
Russell, K
Safouris, V
Wakamatsu, K
Westra, E
Williams, M
AF Jones, D. Heath
Read, Mike A.
Saunders, Will
Colless, Matthew
Jarrett, Tom
Parker, Quentin A.
Fairall, Anthony P.
Mauch, Thomas
Sadler, Elaine M.
Watson, Fred G.
Burton, Donna
Campbell, Lachlan A.
Cass, Paul
Croom, Scott M.
Dawe, John
Fiegert, Kristin
Frankcombe, Leela
Hartley, Malcolm
Huchra, John
James, Dionne
Kirby, Emma
Lahav, Ofer
Lucey, John
Mamon, Gary A.
Moore, Lesa
Peterson, Bruce A.
Prior, Sayuri
Proust, Dominique
Russell, Ken
Safouris, Vicky
Wakamatsu, Ken-ichi
Westra, Eduard
Williams, Mary
TI The 6dF Galaxy Survey: final redshift release (DR3) and southern
large-scale structures
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; galaxies: distances and redshifts; cosmology: observations;
large-scale structure of Universe
ID DIGITAL SKY SURVEY; HOROLOGIUM-RETICULUM SUPERCLUSTER; PROBE WMAP
OBSERVATIONS; SHAPLEY SUPERCLUSTER; LUMINOSITY FUNCTION; SPECTROSCOPY
SYSTEM; STREAMING MOTIONS; GREAT ATTRACTOR; POWER-SPECTRUM;
VELOCITY-FIELD
AB We report the final redshift release of the 6dF Galaxy Survey (6dFGS), a combined redshift and peculiar velocity survey over the southern sky (|b| > 10 degrees). Its 136 304 spectra have yielded 110 256 new extragalactic redshifts and a new catalogue of 125 071 galaxies making near-complete samples with (K, H, J, r(F), b(J)) < (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. Survey data, including images, spectra, photometry and redshifts, are available through an online data base. We describe changes to the information in the data base since earlier interim data releases. Future releases will include velocity dispersions, distances and peculiar velocities for the brightest early-type galaxies, comprising about 10 per cent of the sample. Here we provide redshift maps of the southern local Universe with z < 0.1, showing nearby large-scale structures in hitherto unseen detail. A number of regions known previously to have a paucity of galaxies are confirmed as significantly underdense regions. The URL of the 6dFGS data base is http://www-wfau.roe.ac.uk/6dFGS.
C1 [Jones, D. Heath; Saunders, Will; Colless, Matthew; Parker, Quentin A.; Watson, Fred G.; Burton, Donna; Campbell, Lachlan A.; Cass, Paul; Dawe, John; Fiegert, Kristin; Hartley, Malcolm; James, Dionne; Russell, Ken] Anglo Australian Observ, Epping, NSW 1710, Australia.
[Read, Mike A.] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jarrett, Tom] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Parker, Quentin A.] Macquarie Univ, Dept Phys, Sydney, NSW 2109, Australia.
[Fairall, Anthony P.] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa.
[Mauch, Thomas] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Sadler, Elaine M.; Croom, Scott M.; Moore, Lesa] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Campbell, Lachlan A.; Frankcombe, Leela; Kirby, Emma; Peterson, Bruce A.; Prior, Sayuri; Safouris, Vicky; Westra, Eduard; Williams, Mary] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Huchra, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Lucey, John] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Mamon, Gary A.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Mamon, Gary A.; Proust, Dominique] Observ Paris, CNRS, UMR 8111, GEPI, F-92195 Meudon, France.
[Wakamatsu, Ken-ichi] Gifu Univ, Fac Engn, Gifu 5011193, Japan.
RP Jones, DH (reprint author), Anglo Australian Observ, POB 296, Epping, NSW 1710, Australia.
EM heath@aao.gov.au
RI Frankcombe, Leela/C-7003-2012;
OI Frankcombe, Leela/0000-0001-6578-3200; Sadler,
Elaine/0000-0002-1136-2555; Mamon, Gary/0000-0001-8956-5953; Colless,
Matthew/0000-0001-9552-8075
FU Australian Research Council [DP-0208876]; US National Science Foundation
[AST0406906]
FX DHJ acknowledges support from Australian Research Council Discovery -
Projects Grant (DP-0208876), administered by the Australian National
University. JH acknowledges support from the US National Science
Foundation under grant AST0406906. We also acknowledge the valuable
contributions of an anonymous referee. We dedicate this paper to two
colleagues who made important contributions to the 6dFGS before their
passing: John Dawe (1942-2004), observer and long-time proponent of
wide-field fibre spectroscopy on the UKST from its earliest days, and
Tony Fairall (1943-2008), whose unique insights from a career-long
dedication to mapping the southern Universe underpin much of the
interpretation contained herein.
NR 72
TC 287
Z9 288
U1 1
U2 9
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 OCT 21
PY 2009
VL 399
IS 2
BP 683
EP 698
DI 10.1111/j.1365-2966.2009.15338.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 505AW
UT WOS:000270661300015
ER
PT J
AU Fittingoff, A
Prochaska, JX
Kalirai, JS
Strader, J
Guhathakurta, P
Kaplan, KF
AF Fittingoff, Andrew
Prochaska, J. Xavier
Kalirai, Jasonjot S.
Strader, Jay
Guhathakurta, Puragra
Kaplan, Kyle F.
TI A survey of ultraviolet-bright sources behind the halo of M31
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: haloes; galaxies: individual: M31; quasars: absorption lines
ID GIANT SOUTHERN STREAM; GALAXY FORMATION; MINOR AXIS; ANDROMEDA;
KINEMATICS; ABSORBERS; DISCOVERY; CONSTRAINTS; REDSHIFTS; CLUSTERS
AB We have performed a wide-area ultraviolet (UV) imaging survey using the GALaxy Evolution eXplorer to search for bright, point-like UV sources behind M31's extended halo. Our survey consisted of 46 pointings covering an effective area of approximate to 50 deg2, in both the far-UV and near-UV channels. We combined these data with optical R-band observations acquired with the WIYN Mosaic-1 imager on the Kitt Peak National Observatory 0.9-m WIYN telescope. An analysis of the brightness and colours of sources matched between our photometric catalogues yielded approximate to 100 UV-bright quasar candidates. We have obtained discovery spectra for 76 of these targets with the Kast spectrometer on the Lick 3-m telescope and confirmed 30 active galactic nuclei and quasars, 29 galaxies at z > 0.02 including several early-type systems, 16 Galactic stars (hot main-sequence stars) and one featureless source previously identified as a BL Lac object. Future UV spectroscopy of the brightest targets with the Cosmic Origins Spectrograph on the Hubble Space Telescope will enable a systematic search for diffuse gas in the extended halo of M31.
C1 [Fittingoff, Andrew; Prochaska, J. Xavier; Strader, Jay; Guhathakurta, Puragra; Kaplan, Kyle F.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Prochaska, J. Xavier; Kalirai, Jasonjot S.; Guhathakurta, Puragra] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Kalirai, Jasonjot S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fittingoff, A (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM andrewf@sfsu.edu
FU NASA [NNG06GD37G, NAS5-26555]; NSF [AST-0607852]
FX AF, JXP, JSK and PG acknowledge support from NASA grant NNG06GD37G, as
part of the GALEX GO programme. PG and JSK acknowledge support from NSF
grant AST-0607852. J S was supported by NASA through a Hubble
Fellowship, administered by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555.
NR 34
TC 2
Z9 2
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2009
VL 399
IS 2
BP 728
EP 736
DI 10.1111/j.1365-2966.2009.15370.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 505AW
UT WOS:000270661300018
ER
PT J
AU Longmore, SN
Burton, MG
Keto, E
Kurtz, S
Walsh, AJ
AF Longmore, S. N.
Burton, M. G.
Keto, E.
Kurtz, S.
Walsh, A. J.
TI Too large and overlooked ? Extended free-free emission towards massive
star formation regions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: early-type; stars: evolution; stars: formation; ISM: evolution; H
ii regions; radio continuum: ISM; radio lines: ISM
ID RADIO-CONTINUUM EMISSION; H II REGIONS; METHANOL MASERS;
HIGH-RESOLUTION; HOT CORES
AB We present Australia Telescope Compact Array observations towards six massive star formation regions, which, from their strong 24 GHz continuum emission but no compact 8 GHz continuum emission, appeared good candidates for hypercompact H ii regions. However, the properties of the ionized gas derived from the 19 to 93 GHz continuum emission and H70 alpha + H57 alpha radio recombination line data show the majority of these sources are, in fact, regions of spatially extended, optically thin free-free emission. These extended sources were missed in the previous 8 GHz observations due to a combination of spatial filtering, poor surface brightness sensitivity and primary beam attenuation.
We consider the implications that a significant number of these extended H ii regions may have been missed by previous surveys of massive star formation regions. If the original sample of 21 sources is representative of the population as a whole, the fact that six contain previously undetected extended free-free emission suggests a large number of regions have been mis-classified. Rather than being very young objects prior to UCH ii region formation, they are, in fact, associated with extended H ii regions and thus significantly older. In addition, inadvertently ignoring a potentially substantial flux contribution (up to similar to 0.5 Jy) from free-free emission has implications for dust masses derived from sub-mm flux densities. The large spatial scales probed by single-dish telescopes, which do not suffer from spatial filtering, are particularly susceptible and dust masses may be overestimated by up to a factor of similar to 2.
C1 [Longmore, S. N.; Keto, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Longmore, S. N.; Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Longmore, S. N.] CSIRO, Australia Telescope Natl Facil, Sydney, NSW 1710, Australia.
[Kurtz, S.] Univ Nacl Autonoma Mexico, CRyA, Morelia 58089, Michoacan, Mexico.
[Walsh, A. J.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia.
RP Longmore, SN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM slongmore@cfa.harvard.edu
RI Walsh, Andrew/B-5627-2013;
OI Walsh, Andrew/0000-0001-9506-0855; Burton, Michael/0000-0001-7289-1998
FU Commonwealth of Australia for operation as a National Facility
FX We thank Paul Ho and the referee, Stuart Lumsden, for instructive
comments. The Australia Telescope is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.
NR 17
TC 6
Z9 6
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2009
VL 399
IS 2
BP 861
EP 877
DI 10.1111/j.1365-2966.2009.15320.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 505AW
UT WOS:000270661300032
ER
PT J
AU Li, HB
Dowell, CD
Goodman, A
Hildebrand, R
Novak, G
AF Li, Hua-Bai
Dowell, C. Darren
Goodman, Alyssa
Hildebrand, Roger
Novak, Giles
TI ANCHORING MAGNETIC FIELD IN TURBULENT MOLECULAR CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: magnetic fields; polarization; stars: formation;
turbulence
ID SUBMILLIMETER POLARIZATION; STAR-FORMATION; CORES; ALIGNMENT; DENSITY;
REGIONS; MODELS; DR21
AB One of the key problems in star formation research is to determine the role of magnetic fields. Starting from the atomic intercloud medium which has density n(H) similar to 1 cm(-3), gas must accumulate from a volume several hundred pc across in order to form a typical molecular cloud. Star formation usually occurs in cloud cores, which have linear sizes below 1 pc and densities n(H2) > 10(5) cm(-3). With current technologies, it is hard to probe magnetic fields at scales lying between the accumulation length and the size of cloud cores, a range corresponds to many levels of turbulent eddy cascade, and many orders of magnitude of density amplification. For field directions detected from the two extremes, however, we show here that a significant correlation is found. Comparing this result with molecular cloud simulations, only the sub-Alfvenic cases result in field orientations consistent with our observations.
C1 [Li, Hua-Bai; Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dowell, C. Darren] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Hildebrand, Roger] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hildebrand, Roger] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Dowell, C. Darren] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Hildebrand, Roger] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
RP Li, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
EM hli@cfa.harvard.edu
RI Goodman, Alyssa/A-6007-2010
OI Goodman, Alyssa/0000-0003-1312-0477
FU Smithsonian Astrophysics Observatory; NSF [AST-0505124, AST-0540882]
FX We appreciate the referee, whose comments have made our article much
better. We are grateful to T. K. Sridharan, Zhi-Yun Li, Paolo Padoan,
Telemachos Ch. Mouschovias, Yasuo Fukui, Alex Lazarian, and John Scalo
for insightful discussions and comments. H. L. appreciates the helps
from Tingting Wu on collecting and preliminarily analyzing the optical
data. We thank Scott Paine and Robert Kimberk for proofreading many
versions of themanuscript. H. L.'s research is funded through a
postdoctoral fellowship from the Smithsonian Astrophysics Observatory.
R. H. acknowledges NSF grant AST-0505124 for support of the
submillimeter observations. The Caltech Submillimeter Observatory is
funded through the NSF grant AST-0540882.
NR 38
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 891
EP 897
DI 10.1088/0004-637X/704/2/891
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200058
ER
PT J
AU Sand, DJ
Olszewski, EW
Willman, B
Zaritsky, D
Seth, A
Harris, J
Piatek, S
Saha, A
AF Sand, David J.
Olszewski, Edward W.
Willman, Beth
Zaritsky, Dennis
Seth, Anil
Harris, Jason
Piatek, Slawomir
Saha, Abi
TI THE STAR FORMATION HISTORY AND EXTENDED STRUCTURE OF THE HERCULES MILKY
WAY SATELLITE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; Local Group
ID DWARF SPHEROIDAL GALAXY; DIGITAL SKY SURVEY; SMALL-MAGELLANIC-CLOUD;
STELLAR POPULATION; PHOTOMETRIC SYSTEMS; THEORETICAL ISOCHRONES;
URSA-MAJOR; CLUSTERS; SAGITTARIUS; METALLICITY
AB We present imaging of the recently discovered Hercules Milky Way satellite and its surrounding regions to study its structure, star formation history and to thoroughly search for signs of disruption. We robustly determine the distance, luminosity, size, and morphology of Hercules utilizing a bootstrap approach to characterize our uncertainties. We derive a distance to Hercules via a comparison to empirical and theoretical isochrones, finding a best match with the isochrone of M92, which yields a distance of 133 +/- 6 kpc. As previous studies have found, Hercules is very elongated, with epsilon = 0.67 +/- 0.03 and a half-light radius of r(h) similar or equal to 230 pc. Using the color-magnitude-fitting package StarFISH, we determine that Hercules is old (> 12 Gyr) and metal-poor ([Fe/H] similar to -2.0), with a spread in metallicity, in agreement with previous spectroscopic work. This result is robust with respect to slight variations in the distance to Hercules and mismatches between the observed Hercules color-magnitude diagram and theoretical isochrones. We infer a total absolute magnitude of M(V) = -6.2 +/- 0.4. Our innovative search for external Hercules structure both in the plane of the sky and along the line of sight yields some evidence that Hercules is embedded in a larger stream of stars. A clear stellar extension is seen to the northwest with several additional candidate stellar overdensities along the position angle of Hercules out to similar to 35' (similar to 1.3 kpc). While the association of any of the individual stellar overdensities with Hercules is difficult to determine, we do show that the summed color-magnitude diagram of all three is consistent with Hercules' stellar population. Finally, we estimate that any change in the distance to Hercules across its face is at most similar to 6 kpc, and the data are consistent with Hercules being at the same distance throughout.
C1 [Sand, David J.; Seth, Anil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Olszewski, Edward W.; Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Willman, Beth] Haverford Coll, Dept Astron, Haverford, PA 19041 USA.
[Harris, Jason; Saha, Abi] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Piatek, Slawomir] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
RP Sand, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dave.j.sand@gmail.com
FU NSF [AST-0505711, 0807498, AST-0307492]; NASA LTSA [NNG05GE82G]
FX Many thanks to the LBC SDT team and the Arizona LBT Queue run observers.
John Hill and Olga Kuhn were essential in our obtaining our Hercules
data. We thank Ben Weiner and Michael Cooper for taking extra care when
performing some of these observations. We are grateful to Josh Simon and
Marla Geha for providing their kinematic data on Hercules for this
paper. Also, we are grateful to John Moustakas who provided an initial
version of his LBC reduction code. E. O. was partially supported by NSF
grants AST-0505711 and 0807498. D. Z. acknowledges support from NASA
LTSA award NNG05GE82G and NSF grant AST-0307492.
NR 58
TC 48
Z9 48
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 898
EP 914
DI 10.1088/0004-637X/704/2/898
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200059
ER
PT J
AU Latham, DW
Bakos, GA
Torres, G
Stefanik, RP
Noyes, RW
Kovacs, G
Pal, A
Marcy, GW
Fischer, DA
Butler, RP
Sipocz, B
Sasselov, DD
Esquerdo, GA
Vogt, SS
Hartman, JD
Kovacs, G
Lazar, J
Papp, I
Sari, P
AF Latham, David W.
Bakos, Gaspar A.
Torres, Guillermo
Stefanik, Robert P.
Noyes, Robert W.
Kovacs, Geza
Pal, Andras
Marcy, Geoffrey W.
Fischer, Debra A.
Butler, R. Paul
Sipocz, Brigitta
Sasselov, Dimitar D.
Esquerdo, Gilbert A.
Vogt, Steven S.
Hartman, Joel D.
Kovacs, Gabor
Lazar, Jozsef
Papp, Istvan
Sari, Pal
TI DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet
FIELD G205
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-8, GSC 02757-01152);
techniques: spectroscopic
ID EXTRASOLAR GIANT PLANETS; HOT JUPITER; SPECTROSCOPIC BINARIES;
RADIAL-VELOCITIES; MASSIVE PLANET; LIGHT CURVES; BRIGHT STAR; K-DWARF;
STELLAR; ALGORITHM
AB We report the discovery of HAT-P-8b, a transiting planet with mass M(p) = 1.52(-0.16)(+0.18) M(J), radius R(p) = 1.50(-0.06)(+0.08) R(J), and photometric period P = 3.076 days. HAT-P-8b has a somewhat inflated radius for its mass, and a somewhat large mass for its period. The host star is a solar-metallicity F dwarf, with mass M(*) = 1.28 +/- 0.04 M(circle dot) and R(*) = 1.52(-006)(+0.18) R(circle dot). HAT-P-8b was initially identified as one of the 32 transiting-planet candidates in HATNet field G205. We describe the procedures that we have used to follow up these candidates with spectroscopic and photometric observations, and we present a status report on our interpretation for 28 of the candidates. Eight are eclipsing binaries with orbital solutions whose periods are consistent with their photometric ephemerides; two of these spectroscopic orbits are single-lined and six are double-lined.
C1 [Latham, David W.; Bakos, Gaspar A.; Torres, Guillermo; Stefanik, Robert P.; Noyes, Robert W.; Pal, Andras; Sipocz, Brigitta; Sasselov, Dimitar D.; Esquerdo, Gilbert A.; Hartman, Joel D.; Kovacs, Gabor] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Pal, Andras; Sipocz, Brigitta] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fischer, Debra A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Butler, R. Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Vogt, Steven S.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Lazar, Jozsef; Papp, Istvan; Sari, Pal] Hungarian Astron Assoc, Budapest, Hungary.
RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Butler, Robert/B-1125-2009;
OI Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861
FU NASA [NNG04GN74G, NNX08AF23G, HST-HF-01170.01-A, NNG04LG89G]; SAO IR D;
NSF Astronomy and Astrophysics Program; Kepler Mission under NASA
Cooperative Agreement [NCC2-1390]; Hungarian Scientific Research
Foundation ( OTKA) [K-60750]
FX HATNet operations have been funded by NASA grants NNG04GN74G,
NNX08AF23G, and SAO IR& D grants. Work by G.A.B. was supported by NASA
through Hubble Fellowship Grant HST-HF-01170.01-A and by the
Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program.
We also acknowledge partial support from the Kepler Mission under NASA
Cooperative Agreement NCC2-1390 ( PI: D. W. L.). G. T. acknowledges
partial support from NASA under grant NNG04LG89G, G. K. thanks the
Hungarian Scientific Research Foundation ( OTKA) for support through
grant K-60750. This research has made use of Keck telescope time granted
through NOAO ( program A285Hr). This paper benefited from the comments
of the referee.
NR 49
TC 55
Z9 56
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1107
EP 1119
DI 10.1088/0004-637X/704/2/1107
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200008
ER
PT J
AU Tang, SM
Grindlay, J
AF Tang, Sumin
Grindlay, Jonathan
TI THE QUASAR SDSS J153636.22+044127.0: A DOUBLE-PEAKED EMITTER IN A
CANDIDATE BINARY BLACK HOLE SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; quasars: individual (SDSS
J153636.22+044127.0)
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; H-BETA PROFILES; FE II
EMISSION; ACCRETION DISKS; GAS DISCS; ARP 102B; VARIABILITY; GALAXIES;
MASSES
AB Double-peaked emission lines are believed to be originated from accretion disks around supermassive black holes (SMBHs), and about 3% of z < 0.33 active galactic nuclei (AGNs) are found to be double-peaked emitters. The quasar SDSS J153636.22+044127.0 has recently been identified with peculiar broad-line emission systems exhibiting multiple redshifts. We decompose the H alpha and H beta profiles into a circular Keplerian diskline component and other Gaussian components. We propose that the system is both a double-peaked emitter and a binary SMBH system, where the extra flux in the blue peaks of the broad lines comes from the region around the secondary black hole. We suggest that such black hole binary systems might also exist in many known double-peaked emitters, where the tidal torques from the secondary black hole clear the outer region of the disk around the primary black hole, similar to the gap in a protostellar disk due to the process of planetary migration, and might also stimulate the formation of a vertical extended source in the inner region around the primary which illuminates the disk. However, most secondary SMBHs in such systems might be too small to maintain a detectable broad-line region (BLR), so that the disk line from the primary dominates.
C1 [Tang, Sumin; Grindlay, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tang, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM stang@cfa.harvard.edu
NR 60
TC 21
Z9 21
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1189
EP 1194
DI 10.1088/0004-637X/704/2/1189
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200014
ER
PT J
AU Wang, JF
Fabbiano, G
Karovska, M
Elvis, M
Risaliti, G
Zezas, A
Mundell, CG
AF Wang, Junfeng
Fabbiano, G.
Karovska, M.
Elvis, M.
Risaliti, G.
Zezas, A.
Mundell, C. G.
TI THE HIGHEST RESOLUTION CHANDRA VIEW OF PHOTOIONIZATION AND JET-CLOUD
INTERACTION IN THE NUCLEAR REGION OF NGC 4151
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 4151); galaxies: jets; galaxies: Seyfert;
X-rays: galaxies
ID NARROW-LINE REGION; SEYFERT-GALAXY NGC-4151; HUBBLE-SPACE-TELESCOPE;
ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; NUMERICAL-SIMULATION; PHYSICAL
CONDITIONS; IMAGE-RESTORATION; EXTENDED EMISSION; RADIO STRUCTURES
AB We report high resolution imaging of the nucleus of the Seyfert 1 galaxy NGC 4151 obtained with a 50 ks Chandra High Resolution Camera (HRC) observation. The HRC image resolves the emission on spatial scales of 0.'' 5, similar to 30 pc, showing an extended X-ray morphology overall consistent with the narrow-line region (NLR) seen in optical line emission. Removal of the bright point-like nuclear source and image deconvolution techniques both reveal X-ray enhancements that closely match the substructures seen in the Hubble Space Telescope [O III] image and prominent knots in the radio jet. We find that most of the NLR clouds in NGC 4151 have [O III]/soft X-ray ratio similar to 10, despite the distance of the clouds from the nucleus. This ratio is consistent with the values observed in NLRs of some Seyfert 2 galaxies, which indicates a uniform ionization parameter even at large radii and a density decreasing as r(-2) as expected for a nuclear wind scenario. The [O III]/X-ray ratios at the location of radio knots show an excess of X-ray emission, suggesting shock heating in addition to photoionization. We examine various mechanisms for the X-ray emission and find that, in contrast to jet-related X-ray emission in more powerful active galactic nucleus, the observed jet parameters in NGC 4151 are inconsistent with synchrotron emission, synchrotron self-Compton, inverse Compton of cosmic microwave background photons or galaxy optical light. Instead, our results favor thermal emission from the interaction between radio outflow and NLR gas clouds as the origin for the X-ray emission associated with the jet. This supports previous claims that frequent jet-interstellar medium interaction may explain why jets in Seyfert galaxies appear small, slow, and thermally dominated, distinct from those kpc-scale jets in the radio galaxies.
C1 [Wang, Junfeng; Fabbiano, G.; Karovska, M.; Elvis, M.; Risaliti, G.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mundell, C. G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM juwang@cfa.harvard.edu; gfabbiano@cfa.harvard.edu;
mkarovska@cfa.harvard.edu; elvis@cfa.harvard.edu;
risaliti@cfa.harvard.edu; azezas@cfa.harvard.edu; cgm@astro.livjm.ac.uk
RI Wang, Junfeng/A-1476-2011; Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X
FU NASA [GO8-9101X, NAS8-39073]
FX We thank the anonymous referee for useful comments that improved the
clarity of our paper. This work is partially supported from NASA grant
GO8-9101X and NASA contract NAS8-39073 (CXC). We are grateful to Dan
Harris and Aneta Siemiginowska for their stimulating discussion on radio
jets. J. W. thanks E. Galle and M. Juda ( CXC) for technical assistance
in HRC data reduction.
NR 63
TC 11
Z9 11
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1195
EP 1203
DI 10.1088/0004-637X/704/2/1195
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200015
ER
PT J
AU Hughes, AM
Wilner, DJ
Cho, J
Marrone, DP
Lazarian, A
Andrews, SM
Rao, R
AF Hughes, A. Meredith
Wilner, David J.
Cho, Jungyeon
Marrone, Daniel P.
Lazarian, Alexandre
Andrews, Sean M.
Rao, Ramprasad
TI STRINGENT LIMITS ON THE POLARIZED SUBMILLIMETER EMISSION FROM
PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems: protoplanetary disks;
polarization; stars: individual (HD 163296, TW Hydrae)
ID T-TAURI STARS; MAGNETIC-FIELDS; DUST EMISSION; INTERSTELLAR GRAINS;
RADIATIVE TORQUES; ACCRETION DISKS; CIRCUMSTELLAR DISK; HYDRAE
ASSOCIATION; SOLAR NEBULA; ALIGNMENT
AB We present arcsecond-resolution Submillimeter Array (SMA) polarimetric observations of the 880 mu m continuum emission from the protoplanetary disks around two nearby stars, HD 163296 and TW Hydrae. Although previous observations and theoretical work have suggested that a 2%-3% polarization fraction should be common for the millimeter continuum emission from such disks, we detect no polarized continuum emission above a 3 sigma upper limit of 7 mJy in each arcsecond-scale beam, or <1% in integrated continuum emission. We compare the SMA upper limits with the predictions from the exploratory Cho & Lazarian model of polarized emission from T Tauri disks threaded by toroidal magnetic fields, and rule out their fiducial model at the similar to 10 sigma level. We explore some potential causes for this discrepancy, focusing on model parameters that describe the shape, magnetic field alignment, and size distribution of grains in the disk. We also investigate related effects like the magnetic field strength and geometry, scattering off of large grains, and the efficiency of grain alignment, including recent advances in grain alignment theory, which are not considered in the fiducial model. We discuss the impact each parameter would have on the data and determine that the suppression of polarized emission plausibly arises from rounding of large grains, reduced efficiency of grain alignment with the magnetic field, and/or some degree of magnetic field tangling ( perhaps due to turbulence). A poloidal magnetic field geometry could also reduce the polarization signal, particularly for a face-on viewing geometry like the TW Hya disk. The data provided here offer the most stringent limits to-date on the polarized millimeter-wavelength emission from disks around young stars.
C1 [Hughes, A. Meredith; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cho, Jungyeon] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon, South Korea.
[Cho, Jungyeon; Lazarian, Alexandre] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Marrone, Daniel P.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
Natl Taiwan Univ, Inst Astron & Astrophys, Acad Sinica, Condensed Matter Sci & Phys Dept Bldg 7F, Taipei 10617, Taiwan.
RP Hughes, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mhughes@cfa.harvard.edu; dwilner@cfa.harvard.edu; jcho@cnu.ac.kr;
dmarrone@oddjob.uchicago.edu; lazarian@astro.wisc.edu;
sandrews@cfa.harvard.edu; rrao@asiaa.sinica.edu.tw
OI Marrone, Daniel/0000-0002-2367-1080
FU NASA Origins of Solar Systems Program [NAG5-11777, 5-26555]; National
Science Foundation Graduate Research Fellowship; NASA through Hubble
Fellowship [HF-01203-A]; Space Telescope Science Institute
FX We thank Alyssa Goodman for helpful conversations that improved the
manuscript. Partial support for this work was provided by NASA Origins
of Solar Systems Program Grant NAG5-11777. A. M. H. acknowledges support
from a National Science Foundation Graduate Research Fellowship. Support
for S. M. A. was provided by NASA through Hubble Fellowship grant no.
HF-01203-A awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS 5-26555.
NR 67
TC 26
Z9 26
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1204
EP 1217
DI 10.1088/0004-637X/704/2/1204
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200016
ER
PT J
AU Attrill, GDR
Engell, AJ
Wills-Davey, MJ
Grigis, P
Testa, P
AF Attrill, Gemma D. R.
Engell, Alexander J.
Wills-Davey, Meredith J.
Grigis, Paolo
Testa, Paola
TI HINODE/XRT AND STEREO OBSERVATIONS OF A DIFFUSE CORONAL "WAVE"-CORONAL
MASS EJECTION-DIMMING EVENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: coronal mass ejections (CMEs); Sun: magnetic fields;
Sun: UV radiation; Sun: X-rays, gamma rays
ID ULTRAVIOLET IMAGING TELESCOPE; CME-RELATED DIMMINGS; 1997 MAGNETIC
CLOUD; SOLAR-FLARE WAVES; X-RAY TELESCOPE; EIT WAVES; MORETON WAVE;
PROPAGATING DISTURBANCE; SOHO/EIT OBSERVATIONS; SHOCK-WAVES
AB We report on observations of the first diffuse coronal wave detected by Hinode/XRT. The event occurred near the west solar limb on 2007 May 23, originating from active region (AR) 10956 and was associated with a coronal mass ejection (CME) and coronal dimmings. The bright emission forming the coronal wave expanded predominantly to the east and south of the AR. We use X-Ray Telescope (XRT) and STEREO Behind (B) data combined with a potential magnetic field extrapolation to derive an understanding of the global magnetic field connectivity. We attribute the brightening to the east of the AR to compression and channeling of the plasma along large-scale loops. The brightening to the south of the AR expands across the quiet Sun, making the southern component a likely candidate for identification as a diffuse coronal wave. We analyze the bright front in STEREO/EUVI (B) 171, 195, and 284 angstrom images, as well as in XRT data, finding the strongest components to be largely cospatial in all bandpasses. We also exploit the near-limb location of this event by combining STEREO/COR1 and Extreme Ultra-Violet Imaging Telescope (EUVI) data. Using all the data, we derive a full picture of the low-coronal development of the eruption. The COR1 data show that the southernmost outer edge of the CME is progressively displaced southward during the expansion. EUVI data below the COR1 occulting disk show that the CME is significantly distorted in the low corona as a result of the associated filament eruption. The core coronal dimmings map to the core of the CME; the secondary coronal dimmings map to the CME cavity; and the diffuse coronal wave maps to the outermost edge of the expanding CME shell. The analysis of this near-limb event has important implications for understanding earlier eruptions originating from the same AR on 2007 May 16, 19, and 20.
C1 [Attrill, Gemma D. R.; Engell, Alexander J.; Wills-Davey, Meredith J.; Grigis, Paolo; Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Attrill, GDR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [NNX09AB11G, NNM07AB07C]
FX We sincerely thank the referee for a careful reading of the manuscript
and for their helpful comments, which clarified this work. We are
grateful to Aad van-Ballegooijen, Ed Deluca, and Anthony Yeates for
helpful discussions. We also thank Henry (Trae) Winter for software
assistance and KathyReeves for valuable discussion regarding Hinode/XRT
observations. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC
(UK) as international partners. Scientific operation of the Hinode
mission is conducted by the Hinode science team organized at ISAS/ JAXA.
This team mainly consists of scientists from institutes in the partner
countries. Support for the postlaunch operation is provided by JAXA and
NAOJ ( Japan), STFC ( U. K.), NASA, ESA, and NSC ( Norway). The
STEREO/SECCHI data are produced by an international consortium: NRL,
LMSAL, NASA, GSFC ( USA); RAL ( UK); MPS ( Germany); CSL ( Belgium); and
IOTA, IAS ( France). SOHO is a project of international cooperation
between ESA & NASA. SOLIS data used here are produced cooperatively by
the NSF/NSO and NASA/LWS. This research has made use of NASA's
AstrophysicsData System Bibliographic Services. We acknowledge NASA
grants NNX09AB11G and NNM07AB07C which supported this work.
NR 92
TC 36
Z9 36
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1296
EP 1308
DI 10.1088/0004-637X/704/2/1296
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200023
ER
PT J
AU Owers, MS
Nulsen, PEJ
Couch, WJ
Markevitch, M
AF Owers, Matt S.
Nulsen, Paul E. J.
Couch, Warrick J.
Markevitch, Maxim
TI A HIGH FIDELITY SAMPLE OF COLD FRONT CLUSTERS FROM THE CHANDRA ARCHIVE
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies: clusters: individual (1E0657-558, Abell 1758N, MS1455.0+2232
Abell 2069, Abell 2142, Abell 2163, RXJ1720.1+2638, Abell 3667, Abell
665, Abell 2034); X-rays: galaxies: clusters
ID XMM-NEWTON OBSERVATIONS; X-RAY-CLUSTER; EXTENDED RADIO-EMISSION; HOTTEST
KNOWN CLUSTER; GALAXY CLUSTER; DARK-MATTER; ABELL 3667; MERGING
CLUSTERS; 1E 0657-56; TEMPERATURE STRUCTURE
AB This paper presents a sample of "cold front" clusters selected from the Chandra archive. The clusters are selected based purely on the existence of surface brightness edges in their Chandra images which are modeled as density jumps. A combination of the derived density and temperature jumps across the fronts is used to select nine robust examples of cold front clusters: 1ES0657-558, Abell 1201, Abell 1758N, MS1455.0+2232, Abell 2069, Abell 2142, Abell 2163, RXJ1720.1+2638, and Abell 3667. This sample is the subject of an ongoing study aimed at relating cold fronts to cluster merger activity, and understanding how the merging environment affects the cluster constituents. Here, temperature maps are presented along with the Chandra X-ray images. A dichotomy is found in the sample in that there exists a subsample of cold front clusters which are clearly mergers based on their X-ray morphologies, and a second subsample of clusters which harbor cold fronts, but have surprisingly relaxed X-ray morphologies, and minimal evidence for merger activity at other wavelengths. For this second subsample, the existence of a cold front provides the sole evidence for merger activity at X-ray wavelengths. We discuss how cold fronts can provide additional information which may be used to constrain merger histories, and also the possibility of using cold fronts to distinguish major and minor mergers.
C1 [Owers, Matt S.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Owers, Matt S.; Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Nulsen, Paul E. J.; Markevitch, Maxim] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Owers, MS (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM mowers@astro.swin.edu.au
OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493
FU Australian Postgraduate Award; Australian Research Council; NASA
[NAS8-03060]
FX We thank the anonymous referee for useful comments which greatly
improved this manuscript. M.S.O. was supported by an Australian
Postgraduate Award, and acknowledges the hospitality of the
Harvard-Smithsonian Center for Astrophysics where a major portion of
this study was undertaken. We acknowledge the financial support of the
Australian Research Council (via its Discovery Project Scheme)
throughout the course of this work. P.E.J.N. was supported by NASA grant
NAS8-03060. This research has made use of software provided by the
Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and
Sherpa and also of data obtained from the Chandra archive at the NASA
Chandra X-ray center (http://cxc.harvard.edu/cda/). 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 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.
NR 101
TC 58
Z9 58
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1349
EP 1370
DI 10.1088/0004-637X/704/2/1349
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200028
ER
PT J
AU Xu, YD
Chen, XL
Fan, ZH
Trac, H
Cen, RY
AF Xu, Yidong
Chen, Xuelei
Fan, Zuhui
Trac, Hy
Cen, Renyue
TI THE 21 cm FOREST AS A PROBE OF THE REIONIZATION AND THE TEMPERATURE OF
THE INTERGALACTIC MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; intergalactic medium; quasars: absorption lines
ID SIMULATING COSMIC REIONIZATION; HIGH-REDSHIFT; HYDROGEN REIONIZATION;
CENTIMETER TOMOGRAPHY; ABSORPTION-SPECTRA; BUBBLE-GROWTH; LARGE SCALES;
DARK-AGES; EMISSION; MINIHALOS
AB Using high-redshift radio sources as background, the 21 cm forest observations probe the neutral hydrogen absorption signatures of early structures along the lines of sight. Directly sensitive to the spin temperature of the hydrogen atoms, it complements the 21 cm tomography observations, and provides information on the temperature as well as the ionization state of the intergalactic medium (IGM). We use a radiative transfer simulation to investigate the 21 cm forest signals during the epoch of reionization. We first confirmed that the optical depth and equivalent width (EW) are good representations of the ionization and thermal state of the IGM. The features selected by their relative optical depth are excellent tracers of ionization fields, and the features selected by their absolute optical depth are very sensitive to the IGM temperature, so the IGM temperature information could potentially be extracted from 21 cm forest observation, thus breaking a degeneracy in 21 cm tomographic observation. With the EW statistics, we predict some observational consequences for 21 cm forest. From the distributions of EWs and the number evolution of absorbers and leakers with different EWs, we see clearly the cosmological evolution of ionization state of the IGM. The number density of potentially observable features decreases rapidly with increasing gas temperature. The sensitivity of the proposed EW statistic to the IGM temperature makes it a unique and potentially powerful probe of reionization. Missing small-scale structures, such as small filaments and minihalos that are unresolved in our current simulation, and lack of an accurate calculation of the IGM temperature, however, likely have rendered the presented signals quantitatively inaccurate. Finally, we discuss the requirements of the background radio sources for such observations, and find that signals with equivalent widths larger than 1 kHz are hopeful to be detected.
C1 [Xu, Yidong; Fan, Zuhui] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China.
[Xu, Yidong; Chen, Xuelei] CAS, Natl Astron Observ China, Beijing 100012, Peoples R China.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cen, Renyue] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Xu, YD (reprint author), Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China.
RI Trac, Hy/N-8838-2014
OI Trac, Hy/0000-0001-6778-3861
FU NSFC [10525314, 10503010, 10373001, 10773001]; CAS [KJCX3-SYW-N2]; MoST
973 grant [2007CB815401]; NASA ATP [NNG06GI09G]
FX We thank Bin Yue, Andrea Ferrara, Steven Furlanetto and Chris Carilli
for helpful discussion. This research is supported in part by the NSFC
grant 10525314, 10503010, 10373001, 10773001, by the CAS grant
KJCX3-SYW-N2, MoST 973 grant 2007CB815401, and by NASA ATP grant
NNG06GI09G. Computing resources were in part provided by the NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
NR 35
TC 11
Z9 11
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1396
EP 1404
DI 10.1088/0004-637X/704/2/1396
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200031
ER
PT J
AU Takahashi, S
Ho, PTP
Tang, YW
Kawabe, R
Saito, M
AF Takahashi, Satoko
Ho, Paul T. P.
Tang, Ya-Wen
Kawabe, Ryohei
Saito, Masao
TI EVOLUTIONARY STATUS OF BRIGHTEST AND YOUNGEST SOURCE IN THE ORION
MOLECULAR CLOUD-3 REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: evolution; ISM: individual (OMC3-MMS6); radio
continuum: stars; stars: formation
ID SUBMILLIMETER-WAVE OBSERVATIONS; MASS STAR-FORMATION; PROTOSTELLAR
COLLAPSE; INITIAL CONDITIONS; DENSITY STRUCTURE; MILLIMETER ARRAY;
OMC-2/3 REGION; TAURUS-AURIGA; STELLAR CORES; 1ST CORES
AB The brightest continuum source in the Orion molecular cloud-3 region (OMC-3), MMS 6, was observed with the Very Large Array (VLA), the Nobeyama Millimeter Array (NMA), and the Submillimeter Array (SMA). Our data were supplemented by near-to mid-infrared archival data taken by Spitzer Space Telescope. The compact continuum source, MMS 6-main, was detected with an H(2) mass of 3.0 M(circle dot) with a size of 510 AU. Despite its compact and well-condensed appearance, neither clear CO outflow, radio jet, nor infrared sources (at a wavelength shorter than 8 mu m) were detected at MMS 6-main even with the present high angular resolution and high-sensitivity observations. The derived H(2) column density, 2.6 x 10(25) cm(-2), corresponds to a visual extinction of A(nu) similar to 15,000 mag, and the derived number density is at least two orders of magnitude higher than for the other OMC-2/3 continuum sources. The volume density profile of the source was estimated to have a power-law index of 2 or steeper down to a radius of similar to 450 AU. The timescale to form a protostar at the center or the timescale elapsed after its formation is estimated to be 830 to 7600 yr. This is much shorter than the typical lifetime of the Class 0/I protostars, which is similar to 10(4)-10(5) yr, suggesting that MMS 6-main is probably in either the earliest stage of the protostellar core or in the latest stage of the prestellar phase.
C1 [Takahashi, Satoko; Ho, Paul T. P.; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan.
[Kawabe, Ryohei; Saito, Masao] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Takahashi, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM satoko_t@asiaa.sinica.edu.tw
OI Tang, Ya-Wen/0000-0002-0675-276X
FU MEXT, Japan [18204017]; Japan Society for the Promotion of Science
(JSPS); Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan
FX We acknowledge the staff at the Nobeyama Radio Observatory, the
Submillimeter Array, and the National Radio Astronomy Observatory, for
assistance with operations and data reductions. The authors thank J. Lim
for his early contributions to the VLA observations, and C.-H. Yan for
his support with the infrared data analysis. S. T. is deeply grateful to
L. A. Zapata for the information provided on continuum source data in
the OMC 1-South region. S. T. acknowledges Y. N. Su, B. A. Whitney, K.
Asada, N. Ohashi, W. P. Chen, and J. H. S. Lin for helpful discussions.
We also thank an anonymous referee whose suggestions improved this
manuscript. This publication used archival data from the Spitzer Space
Telescope and the Very Large Array. A part of this study was financially
supported by grant in-aid for Scientific Research 18204017 (or Global
COE Program "the Physical Science Frontier" MEXT, Japan). S. T. was
financially supported by the Japan Society for the Promotion of Science
(JSPS) for Young Scientists, and is financially supported by a
postdoctoral fellowship at the Institute of Astronomy and Astrophysics,
Academia Sinica, Taiwan.
NR 73
TC 10
Z9 10
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1459
EP 1470
DI 10.1088/0004-637X/704/2/1459
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200035
ER
PT J
AU Liu, JF
AF Liu, Jifeng
TI MULTI-EPOCH MULTI-WAVELENGTH STUDY OF AN ULTRALUMINOUS X-RAY SOURCE IN
M101: THE NATURE OF THE SECONDARY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M101); X-rays: binaries
ID MASS BLACK-HOLES; OPTICAL COUNTERPART; SPACED DATA; XMM-NEWTON;
GALAXIES; PERIOD; X-1; DISCOVERY; EMISSION; OUTBURST
AB Ultraluminous X-ray sources are non-nuclear point sources in external galaxies with L(X) = 2 x 10(39)-10(41) erg s(-1), and thus are possibly stellar black holes with special radiation mechanisms or intermediate mass black holes of 100-10(5) M(circle dot). To measure their dynamical mass, one needs to identify the secondary in the optical followed by photometric and spectroscopic monitoring. The counterpart light is usually contaminated, sometimes even dominated, by the X-ray irradiated accretion disk, which complicates the derivation of the properties of the secondary itself. Here, we report a study on M101-ULX1 with 26 Hubble Space Telescope (HST) observations and 33 X-ray observations over 16 years. There were three multi-band HST observations at different optical states over eight years, the spectral energy distributions (SEDs) of which cannot be fitted by the previously claimed secondary of a B supergiant or any other single star. All SEDs can be decomposed into the same stellar component plus a second component due to X-ray irradiation with different contributions at different optical states. The secondary in ULX1 is most likely a WR star as revealed by the SED decompositions and confirmed by the presence of He II lambda 4686 emission in the counterpart spectrum. Five X-ray outbursts and two optical peaks are revealed from X-ray and optical light curves, and optical peaks are identified as the optical response to X-ray outbursts. The correlated optical and X-ray variability analysis is suggestive of ellipsoidal modulation with a half-amplitude of 0.05 mag and a period in the range of 1.5-4.5 days. Future photometric and spectroscopic observations are required to confirm the orbital period and measure the dynamical mass for ULX1.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Liu, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [PF6-70043]; Space Telescope Science Institute [HST-AR-10962.01-A]
FX We thank Jeff McClintock, Albert Kong, Rosanne Di Stefano, and Joel
Bregman for helpful discussions. J.F.L. acknowledges the supports for
this work provided by NASA through the Chandra Fellowship Program (grant
PF6-70043) and through a grant from the Space Telescope Science
Institute (HST-AR-10962.01-A).
NR 42
TC 16
Z9 16
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1628
EP 1639
DI 10.1088/0004-637X/704/2/1628
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200047
ER
PT J
AU Guenther, DB
Kallinger, T
Zwintz, K
Weiss, WW
Kuschnig, R
Casey, MP
Matthews, JM
Moffat, AFJ
Rucinski, SM
Sasselov, D
Walker, GAH
AF Guenther, D. B.
Kallinger, T.
Zwintz, K.
Weiss, W. W.
Kuschnig, R.
Casey, M. P.
Matthews, J. M.
Moffat, A. F. J.
Rucinski, S. M.
Sasselov, D.
Walker, G. A. H.
TI ASTEROSEISMIC ANALYSIS OF THE PRE-MAIN-SEQUENCE STARS IN NGC 2264
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: evolution; stars: pre-main sequence; stars: oscillations; open
clusters and associations: individual (NGC 2264)
ID MASS STARS; EVOLUTION; PROTOSTARS; OPACITIES; CLUSTER; MODEL;
SEISMOLOGY; NGC-6530; TRACKS
AB NGC 2264 is a young open cluster lying above the Galactic plane in which six variable stars have previously been identified as possible pre-main-sequence (PMS) pulsators. Their oscillation spectra are relatively sparse with each star having from 2 to 12 unambiguous frequency identifications based on Microvariability and Oscillations of Stars satellite and multi-site ground-based photometry. We describe our efforts to find classical PMS stellar models (i.e., models evolved from the Hayashi track) whose oscillation spectra match the observed frequencies. We find model eigenspectra that match the observed frequencies and are consistent with the stars' locations in the HR diagram for the three faintest of the six stars. Not all the frequencies found in spectra of the three brightest stars can be matched to classical PMS model spectra possibly because of effects not included in our PMS models such as chemical and angular momentum stratification in the outer layers of the star. All the oscillation spectra contain both radial and nonradial p-modes. We argue that the PMS pulsating stars divide into two groups depending on whether or not they have undergone complete mixing (i.e., have gone through a Hayashi phase). Lower mass stars that do evolve through a Hayashi phase have oscillation spectra predicted by classical PMS models, whereas more massive stars that do not, retain mass infall effects in their surface layers and are not well modeled by classical PMS models.
C1 [Guenther, D. B.; Casey, M. P.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Kallinger, T.; Zwintz, K.; Weiss, W. W.; Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Matthews, J. M.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Observ Astron Mt Megant, Montreal, PQ H3C 3J7, Canada.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Guenther, DB (reprint author), St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
OI Kallinger, Thomas/0000-0003-3627-2561; Zwintz,
Konstanze/0000-0001-9229-8315
FU Natural Sciences and Engineering Research Council of Canada; FQRNT
(Quebec); Austrian Research Promotion Agency (FFG); Austrian Science
Fund [P17580, T 335-N16]
FX The Natural Sciences and Engineering Research Council of Canada supports
the research of D. B. G., J.M.M., A.F.J.M., and S.M.R. A. F.J.M. is also
supported by FQRNT (Quebec). T.K., K.Z., and W. W. W. are supported by
the Austrian Research Promotion Agency (FFG) and the Austrian Science
Fund (FWF; T.K. and W.W.W. through project P17580; KZ through project T
335-N16).
NR 38
TC 10
Z9 10
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2009
VL 704
IS 2
BP 1710
EP 1720
DI 10.1088/0004-637X/704/2/1710
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502UQ
UT WOS:000270486200053
ER
PT J
AU Cohen, O
Drake, JJ
Kashyap, VL
Saar, SH
Sokolov, IV
Manchester, WB
Hansen, KC
Gombosi, TI
AF Cohen, O.
Drake, J. J.
Kashyap, V. L.
Saar, S. H.
Sokolov, I. V.
Manchester, W. B.
Hansen, K. C.
Gombosi, T. I.
TI INTERACTIONS OF THE MAGNETOSPHERES OF STARS AND CLOSE-IN GIANT PLANETS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: coronae
ID HOT JUPITERS; CHROMOSPHERIC ACTIVITY; MAGNETIC-FIELD
AB Since the first discovery of an extrasolar planetary system more than a decade ago, hundreds more have been discovered. Surprisingly, many of these systems harbor Jupiter-class gas giants located close to the central star, at distances of 0.1 AU or less. Observations of chromospheric "hot spots" that rotate in phase with the planetary orbit, and elevated stellar X-ray luminosities, suggest that these close-in planets significantly affect the structure of the outer atmosphere of the star through interactions between the stellar magnetic field and the planetary magnetosphere. Here, we carry out the first detailed three-dimensional magnetohydrodynamics simulation containing the two magnetic bodies and explore the consequences of such interactions on the steady-state coronal structure. The simulations reproduce the observable features of (1) increase in the total X-ray luminosity, (2) appearance of coronal hot spots, and (3) phase shift of these spots with respect to the direction of the planet. The proximate cause of these is an increase in the density of coronal plasma in the direction of the planet, which prevents the corona from expanding and leaking away this plasma via a stellar wind. The simulations produce significant low temperature heating. By including dynamical effects, such as the planetary orbital motion, the simulation should better reproduce the observed coronal heating.
C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.; Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sokolov, I. V.; Manchester, W. B.; Hansen, K. C.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Gombosi, Tamas/G-4238-2011; Hansen, Kenneth/F-3693-2011; Manchester,
Ward/I-9422-2012; Sokolov, Igor/H-9860-2013;
OI Gombosi, Tamas/0000-0001-9360-4951; Hansen, Kenneth/0000-0002-8502-1980;
Sokolov, Igor/0000-0002-6118-0469; Cohen, Ofer/0000-0003-3721-0215
FU NSF [ATM-0823592]; NASA [NNG05GM44G, NAS8-39073]; DoD MURI
FX This work has been inspired by an initial study performed by Noe Lugaz.
We thank an unknown referee for his/her useful comments and Ruth
Murray-Clay for useful discussion. O.C. is supported by NSF-SHINE
ATM-0823592 grant, NASA-LWSTRT Grant NNG05GM44G. J.J.D. and V.L.K. were
funded by NASA contract NAS8-39073 to the Chandra X-ray Center.
Simulation results were obtained using the Space Weather Modelling
Framework, developed by the Canter for Space Environment Modelling, at
the University of Michigan with funding support from NASA ESS, NASA
ESTO-CT, NSF KDI, and DoD MURI.
NR 23
TC 29
Z9 29
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2009
VL 704
IS 2
BP L85
EP L88
DI 10.1088/0004-637X/704/2/L85
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508JR
UT WOS:000270927500003
ER
PT J
AU McQuinn, M
AF McQuinn, Matthew
TI THE IMPLICATIONS OF GUNN-PETERSON TROUGHS IN THE He II Ly alpha FOREST
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE diffuse radiation; intergalactic medium; quasars: absorption lines
ID INTERGALACTIC MEDIUM; REIONIZATION; OPACITY; ABSORPTION; RADIATION;
EVOLUTION; UNIVERSE; HELIUM; Z-SIMILAR-TO-6; QUASARS
AB Many experts believe that the z similar to 3 He II Ly alpha forest will suffer from the same saturation issues as the z similar to 6 H I Ly alpha forest and, therefore, will not be a sensitive probe of He II reionization. However, there are several factors that make He II Ly alpha absorption more sensitive than Hi Ly alpha. We show that observations of He II Ly alpha and Ly beta Gunn-Peterson troughs can provide a relatively model-independent constraint on the volume-averaged He II fraction of x(He II,) (V) greater than or similar to 0.1. This bound derives from first using the most underdense regions in the He II forest to constrain the local He II fraction and, then, assuming photoionization equilibrium with the maximum allowed photoionization rate to calculate the ionization state of nearby gas. It is possible to evade this constraint by a factor of similar to 2, but only if the He II were reionized recently. We argue that He II Ly alpha Gunn-Peterson troughs observed in the spectra of Q0302-003 and HE2347-4342 signify the presence of greater than or similar to 10 comoving Mpc patches in which x(He) (II,) (V) > 0.03. This is a factor of 20 improvement over previous constraints from these spectra and 100 times stronger than the tightest constraint on the Hi volume-filling fraction from the z > 6 H I Lyman forest.
C1 [McQuinn, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McQuinn, Matthew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP McQuinn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mmcquinn@berkeley.edu
NR 21
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2009
VL 704
IS 2
BP L89
EP L92
DI 10.1088/0004-637X/704/2/L89
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508JR
UT WOS:000270927500004
ER
PT J
AU Offner, SSR
Hansen, CE
Krumholz, MR
AF Offner, Stella S. R.
Hansen, Charles E.
Krumholz, Mark R.
TI STELLAR KINEMATICS OF YOUNG CLUSTERS IN TURBULENT HYDRODYNAMIC
SIMULATIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE hydrodynamics; ISM: clouds; ISM: kinematics and dynamics; methods:
numerical; stars: formation; turbulence
ID ORION NEBULA CLUSTER; ADAPTIVE MESH REFINEMENT; MASS STAR-FORMATION;
EARLY SOLAR-SYSTEM; MOLECULAR CLOUDS; DENSE CORES; DECAYING TURBULENCE;
CLUMP DISTRIBUTION; INITIAL CONDITIONS; DRIVEN
AB The kinematics of newly formed star clusters are interesting both as a probe of the state of the gas clouds from which the stars form, and because they influence planet formation, stellar mass segregation, cluster disruption, and other processes controlled in part by dynamical interactions in young clusters. However, to date there have been no attempts to use simulations of star cluster formation to investigate how the kinematics of young stars change in response to variations in the properties of their parent molecular clouds. In this Letter, we report the results of turbulent self-gravitating simulations of cluster formation in which we consider both clouds in virial balance and those undergoing global collapse. We find that stars in these simulations generally have velocity dispersions smaller than that of the gas by a factor of similar to 5, independent of the dynamical state of the parent cloud, so that subvirial stellar velocity dispersions arise naturally even in virialized molecular clouds. The simulated clusters also show large-scale stellar velocity gradients of similar to 0.2-2 km s(-1) pc(-1) and strong correlations between the centroid velocities of stars and gas, both of which are observed in young clusters. We conclude that star clusters should display subvirial velocity dispersions, large-scale velocity gradients, and strong gas-star velocity correlations regardless of whether their parent clouds are in virial balance, and, conversely, that observations of these features cannot be used to infer the dynamical state of the parent gas clouds.
C1 [Offner, Stella S. R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Hansen, Charles E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Offner, Stella S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Offner, SSR (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM soffner@berkeley.edu; chansen@astro.berkeley.edu; krumholz@ucolick.org
OI Krumholz, Mark/0000-0003-3893-854X
FU US Department of Energy [B-542762]; National Science Foundation
[AST-0807739, AST-0901055, UCB267]
FX Support for this work was provided by the US Department of Energy at the
Lawrence Livermore National Laboratory under contract B-542762
(S.S.R.O., C. E. H.), the Alfred P. Sloan Foundation ( M. R. K.),
NASA/JPL through the Spitzer Theoretical Research Program ( M. R. K.),
and the National Science Foundation through grants AST-0807739 ( M. R.
K.) and AST-0901055 ( S.S.R.O.). Computational resources were provided
by the NSF San Diego Supercomputing Center through NPACI program grant
UCB267.
NR 48
TC 40
Z9 40
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 20
PY 2009
VL 704
IS 2
BP L124
EP L128
DI 10.1088/0004-637X/704/2/L124
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508JR
UT WOS:000270927500011
ER
PT J
AU Rueda, LM
Brown, TL
Kim, HC
Klein, TA
Thongkukiatkul, A
Sherwood, V
AF Rueda, Leopoldo M.
Brown, Tracy L.
Kim, Heung-Chul
Klein, Terry A.
Thongkukiatkul, Amporn
Sherwood, Van
TI Description and comparison of morphological structures of the eggs of
Anopheles hyrcanus group and related species (Diptera: Culicidae) from
the Republic of Korea
SO ZOOTAXA
LA English
DT Article
DE Culicidae; Anopheles; mosquito eggs; morphology; Republic of Korea
ID SINENSIS
AB The eggs of six Anopheles Hyrcanus Group (An. sinensis Wiedemann, An. kleini Rueda, An. belenrae Rueda, An. pullus M. Yamada, An. lesteri Baisas and Hu, An. sineroides S. Yamada) and related species (An. koreicus S. Yamada and Watanabe, An. lindesayi japonicus S. Yamada), were described from scanning electron micrographs of specimens collected from different localities of the Republic of Korea. Morphometric measurements of egg samples of the eight species were compared and relationships analyzed by multivariate statistics. About 27 characters were selected and used as a basis for principal and discriminant function analyses. Scanning electron micrographs of various parts of the eggs were selected to illustrate interspecific differences for particular morphological features (e. g. anterior and posterior tubercles, decks, plastron, micropyles, floats).
C1 [Rueda, Leopoldo M.; Brown, Tracy L.; Sherwood, Van] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA.
[Rueda, Leopoldo M.; Brown, Tracy L.] Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, MRC 534, Suitland, MD 20746 USA.
[Kim, Heung-Chul] 65th Med Brigade, Multifunct Med Battal 168, Med Detachment 5, APO, AP 96205 USA.
[Klein, Terry A.] USAMEDDAC Korea, Med Brigade 65, Force Hlth Protect & Prevent Med, APO, AP 96205 USA.
[Thongkukiatkul, Amporn] Burapha Univ, Dept Biol, Chon Buri, Thailand.
RP Rueda, LM (reprint author), Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA.
EM ruedapol@si.edu
RI Valle, Ruben/A-7512-2013
FU Center for Health Promotion and Preventive Medicine; Global Emerging
Infections Surveillance and Response Systems, Silver Spring, MD
FX Funding for this work was provided by the Center for Health Promotion
and Preventive Medicine, Global Emerging Infections Surveillance and
Response Systems, Silver Spring, MD. This research was performed under a
Memorandum of Understanding between the Walter Reed Army Institute of
Research and the Smithsonian Institution, with institutional support
provided by both organizations. The opinions and assertions contained
herein are those of the authors and are not to be construed as official
or reflecting the views of the Department of the Army or the Department
of Defense.
NR 17
TC 2
Z9 2
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 OCT 20
PY 2009
IS 2268
BP 23
EP 40
PG 18
WC Zoology
SC Zoology
GA 508KM
UT WOS:000270929700002
ER
PT J
AU Wilson, LB
Cattell, CA
Kellogg, PJ
Goetz, K
Kersten, K
Kasper, JC
Szabo, A
Meziane, K
AF Wilson, L. B., III
Cattell, C. A.
Kellogg, P. J.
Goetz, K.
Kersten, K.
Kasper, J. C.
Szabo, A.
Meziane, K.
TI Low-frequency whistler waves and shocklets observed at
quasi-perpendicular interplanetary shocks
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTHS BOW SHOCK; AMPLITUDE MAGNETIC-STRUCTURES; COLLISIONLESS SHOCKS;
ISEE-2 OBSERVATIONS; UPSTREAM WAVES; SOLAR-WIND; PARALLEL SHOCK; IONS
UPSTREAM; FORESHOCK; PLASMA
AB We present observations of low-frequency waves (0.25 Hz < f < 10 Hz) at five quasi-perpendicular interplanetary (IP) shocks observed by the Wind spacecraft. Four of the five IP shocks had oblique precursor whistler waves propagating at angles with respect to the magnetic field of 20 degrees-50 degrees and large propagation angles with respect to the shock normal; thus they do not appear to be phase standing. One event, the strongest in our study and likely supercritical, had low-frequency waves consistent with steepened magnetosonic waves called shocklets. The shocklets are seen in association with diffuse ion distributions. Both the shocklets and precursor whistlers are often seen simultaneously with anisotropic electron distributions unstable to the whistler heat flux instability. The IP shock with upstream shocklets showed much stronger electron heating across the shock ramp than the four events without upstream shocklets. These results may offer new insights into collisionless shock dissipation and wave-particle interactions in the solar wind.
C1 [Wilson, L. B., III; Cattell, C. A.; Kellogg, P. J.; Goetz, K.; Kersten, K.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA.
[Kasper, J. C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meziane, K.] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada.
RP Wilson, LB (reprint author), Univ Minnesota, Dept Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM wilson@physics.umn.edu; cattell@fields.space.umn.edu;
pauljkellogg@gmail.com; goetz@umn.edu; kkersten@physics.umn.edu;
jkasper@cfa.harvard.edu; adam.szabo-1@nasa.gov; karim@unb.ca
RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012;
OI Kasper, Justin/0000-0002-7077-930X; Wilson III,
Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X
FU NESSF [NNX07AU72H, NNX07AI05G]
FX [49] Zuyin Pu thanks the reviewers for their assistance in evaluating
this paper.
NR 38
TC 33
Z9 33
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT 17
PY 2009
VL 114
AR A10106
DI 10.1029/2009JA014376
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508PK
UT WOS:000270945100004
ER
PT J
AU Velazco, PM
Gardner, AL
AF Velazco, Paul M.
Gardner, Alfred L.
TI A new species of Platyrrhinus (Chiroptera: Phyllostomidae) from western
Colombia and Ecuador, with emended diagnoses of P. aquilus, P. dorsalis,
and P. umbratus
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB The Neotropical bat genus Platyrrhinus (Chiroptera: Phyllostomidae: Stenodermatinae) currently comprises 15 species. Our morphological and morphometric analysis of large and medium-sized Platyrrhinus revealed a distinctive Undescribed species from western South America. We also recognize P. aquilus (Handley & Ferris 1972) and P. umbratus (Lyon 1902) as valid species. We describe P. nitelinea sp. nov. from western Colombia and Ecuador and provide emended diagnoses along with descriptions of P. aquilus, P.. dorsalis, and P. umbratus. Phylogenetic analysis of Platyrrhinus based on morphological characters indicates that P. aquilus is closely related to P. aurarius and P. nigellus, P. umbratus to P. chocoensis, and P. nitelinea to P. vittatus.
C1 [Velazco, Paul M.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA.
[Velazco, Paul M.] Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA.
[Gardner, Alfred L.] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, MRC 111, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Velazco, PM (reprint author), Field Museum Nat Hist, Dept Zool, 1400 S Lake Shore Dr, Chicago, IL 60605 USA.
EM pvelazco@fieldmuseum.org; gardnera@si.edu
RI Velazco, Paul/K-4186-2012
OI Velazco, Paul/0000-0001-7195-7422
FU NSF [DEB 9870191, OISE 0630149]; American Society of Mammalogists; Ellen
Thorne Smith Fund (FMNH); Barbara E. Brown Fund for Mammal Research
(FMNH); Lester Armour Graduate Fellowship (FMNH); Smithsonian
Institution Pre-doctoral Fellowship; Museum of Comparative Zoology at
Harvard University; University of Illinois at Chicago
FX This study was part of PMV's dissertation submitted to the University of
Illinois at Chicago as partial fulfillment of his doctoral degree. PMV
thanks committee members, M. Ashley, H. F. Howe, R. Mason-Garner, B. D.
Patterson, and R. H. Ree. Special recognition is due to B. D. Patterson
for his constant support and encouragement to PMV. The following
Curators and collection staff graciously provided access to specimens
under their care: Daphne M. Hills and Paula Jenkins (BMNH), Suzanne B.
McLaren (CM), Renato Gregorin (CMUFLA), Bruce D. Patterson and John
Phelps (FMNH), J. Enrique Castillo (IAvH-M), Yaneth Muhoz-Saba (ICN),
Gustavo A. B. da Fonseca, Raquel Texeira de Moura, Valeria C. Tavares,
Yuri Leite, and Leonora Pires Costa (DZ-UFMG); Santiago Madrinan (ULA),
Mark S. Hafner (LSUMZ), Judith Chupasko (MCZ), Ce cile Callou (MNHN),
Carlos Delgado, Javier Munoz, and Danny Zurc (MUA); Victor Pacheco
(MUSM), James L. Patton (MVZ), Judith L. Eger and Burton K. Lim (ROM),
Philip Myers (UMMZ), Linda K. Gordon, James G. Mead (USNM), and Suzanne
C. Peurach (USGS-PWRC); Oscar Murillo Garcia (UV), Hendrik Turni and
Robert Asher (ZMB). Many of the specimens were collected with NSF
support (DEB 9870191 to Bruce D. Patterson and colleagues; OISE 0630149
to BDP and PMV). The research was also supported by a Grant-M-Aid of
Research from the American Society of Mammalogists, and the Ellen Thorne
Smith Fund (FMNH), Barbara E. Brown Fund for Mammal Research (FMNH), the
Lester Armour Graduate Fellowship (FMNH), the Smithsonian Institution
Pre-doctoral Fellowship, Ernest Mayr Travel Grant in Animal Systematics
from the Museum of Comparative Zoology at Harvard University, The Albert
R. and Alma Shadle Fellowship in Mammalogy from the American Society of
Mammalogists, and the Provost's Award for Graduate Research from the
University of Illinois at Chicago. Lastly, we appreciate the
constructive comments that were provided by M. Monica Diaz, Michael D.
Carleton, and one anonymous reviewer.
NR 30
TC 8
Z9 12
U1 1
U2 7
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD OCT 14
PY 2009
VL 122
IS 3
BP 249
EP 281
PG 33
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 511EB
UT WOS:000271145600001
ER
PT J
AU Heyer, WR
Barrio-Amoros, CL
AF Heyer, W. Ronald
Luis Barrio-Amoros, Cesar
TI The advertisement calls of two sympatric frogs, Leptodactylus
lithonaetes (Amphibia: Anura: Leptodactylidae) and Pristimantis vilarsi
(Amphibia: Anura: Strabomantidae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB The advertisement calls of the frog species Leptodactylus lithonaetes and Pristimantis vilarsi are described for the first time based on calls recorded in the Venezuelan State of Amazonas. The call of L. lithonaetes bears an overall resemblance to that of L. rugosus, suggesting a sister-group relationship between the two species. The call of Pristimantis vilarsi is similar to those of other species in the P. conspicillatus species group.
C1 [Heyer, W. Ronald] Smithsonian Inst, Div Amphibians & Reptiles, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Luis Barrio-Amoros, Cesar] Fdn AndigenA, Merida 5101 A, Venezuela.
RP Heyer, WR (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM heyerr@si.edu; cesarlba@yahoo.com
FU NSF [DEB-0342912]
FX Research for this study was Supported by NSF award DEB-0342912 to Rafael
O. de SA and W. Ronald Heyer. CLBA thanks Charles Brewer-Carias and
Goran Safarek for financial support for fieldwork undertaken at the two
localities where the recordings were made.
NR 9
TC 4
Z9 9
U1 0
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
EI 1943-6327
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD OCT 14
PY 2009
VL 122
IS 3
BP 282
EP 291
PG 10
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 511EB
UT WOS:000271145600002
ER
PT J
AU Heyer, WR
Giaretta, AA
AF Heyer, W. Ronald
Giaretta, Ariovaldo A.
TI Advertisement calls, notes on natural history, and distribution of
Leptodactylus chaquensis (Amphibia: Anura: Leptodactylidae) in Brasil
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID SOUTHEASTERN BRAZIL; PARENTAL BEHAVIOR; FROGS; HABITAT; GENUS; SIZE
AB Three types of advertisement calls of Leptodactylus chaquensis from the Cerrado of Minas Gerais, Brasil are described - growls, grunts, and trills. Additional variation includes calls that start with growls and end with trills. The growl call has not been reported previously. Tadpoles are described and agree with previous descriptions. A female was found associated with tadpoles for at least 20 d. The female communicated with the tadpoles by pumping behavior and also exhibited aggressive behavior toward potential predators. The data reported herein are the First conclusive evidence that L. chaquensis occurs in the Cerrado of Minas Gerais. Other reported Brasilian records for L. chaquensis come from the southern portion of the Cerrado. Additional field work is necessary to determine whether L. chaquensis occurs in the northern Cerrado (in the states of Bahia, Distrito Federal, Maranhao, Par, and Tocantins).
C1 [Heyer, W. Ronald] Smithsonian Inst, MRC 162, Washington, DC 20013 USA.
[Giaretta, Ariovaldo A.] Univ Fed Uberlandia, BR-38400902 Uberlandia, MG, Brazil.
RP Heyer, WR (reprint author), Smithsonian Inst, MRC 162, POB 37012, Washington, DC 20013 USA.
EM heyerr@si.edu; thoropa@inbio.ufu.br
FU CNPq; FAPEMIG; NSF [DEB-0342918]
FX Financial grant support to AAG was provided by CNPq and FAPEMIG as well
as a fellowship from CNPq. Wagner R. da Silva, L. B. Martins, D. R. da
Silva, and A. P. Rodrigues helped in the fieldwork. Adir F. Lemos
allowed the field team access to his property and provided facilities.
WRH was supported by NSF award DEB-0342918 to Rafael O. de Sd and WRH.
Miriam Heyer improved the readability of the text. Rafael O. de Sd
critically reviewed the manuscript prior to submission. Reviewers Steve
Gotte and Ignacio De la Riva brought several problems and clarifications
to our attention, significantly improving the paper.
NR 46
TC 8
Z9 8
U1 0
U2 7
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD OCT 14
PY 2009
VL 122
IS 3
BP 292
EP 305
PG 14
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 511EB
UT WOS:000271145600003
ER
PT J
AU Bunwong, S
Robinson, H
Chantaranothai, P
AF Bunwong, Sukhonthip
Robinson, Harold
Chantaranothai, Pranom
TI Taxonomic notes on Camchaya and Iodocephalus (Vernonieae: Asteraceae),
and a new genus Iodocephalopsis
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB The two species originally described in the genus Iodocephalus Gagnep. are not congeneric. The species that was retained in the genus by Kitamura and stated as the type of the genus by Swart is reduced to synonymy under Camchcqa Gagnep., and a new combination Camchaya gracilis (Gagnep.) S. Bunwong & H. Rob. is proposed. This species is reported for the First time from Thailand. A new genus, Iodocephalopsis S. Bunwong & H. Rob., is established for the second species originally placed in Iodocephalus, and both Iodocephalus glandulosus Kerr and Camchaya eberhardtii (Gagnep.) Kitam. are placed in synonymy tinder the newly combined Iodocephalopsis eberhardtii (Gagnep.) S. Bunwong & H. Rob.
C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Bunwong, Sukhonthip; Chantaranothai, Pranom] Khon Kaen Univ, Appl Taxon Res Ctr, Fac Sci, Dept Biol, Khon Kaen 40002, Thailand.
RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM sukhonthipb37@gmail.com; robinsoh@si.edu; pranom@kku.ac.th
FU TRF/BIOTEC [BRT_T151007]; Ministry of Education; Institute for the
Promotion of Teaching Science and Technology (IPST), Thailand
FX This work was supported by the TRF/BIOTEC Special Program for
Biodiversity Research and Training Grant BRT_T151007, and the Ministry
of Education and the Institute for the Promotion of Teaching Science and
Technology (IPST), Thailand. We thank Dr. D. A. Simpson for comments on
the manuscript and also acknowledge the curators and staff of the
following herbaria for access to their facilities: AAU, B, BCU, BK, BKF,
BM, C, CMU, G, I, K, KKU, L, P, QBG and US. Drs. John Strother, Dan
Nicolson. and John McNeil are thanked for comments on the nomenclature.
NR 16
TC 2
Z9 2
U1 1
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD OCT 14
PY 2009
VL 122
IS 3
BP 357
EP 363
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 511EB
UT WOS:000271145600009
ER
PT J
AU Krayesky, DM
Norris, JN
Gabrielson, PW
Gabriel, D
Fredericq, S
AF Krayesky, David M.
Norris, James N.
Gabrielson, Paul W.
Gabriel, Daniela
Fredericq, Suzanne
TI A new order of red algae based on the Peyssonneliaceae, with an
evaluation of the ordinal classification of the Florideophyceae
(Rhodophyta)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Review
ID RNA GENE-SEQUENCES; SMALL-SUBUNIT; RHODYMENIALES RHODOPHYTA;
REPRODUCTIVE MORPHOLOGY; UNCHARTED SEAMOUNT; RIBOSOMAL DNA; NUCLEAR
LARGE; GIGARTINALES; PHYLOGENY; SYSTEMATICS
AB The Peyssonneliaceae Denizot comprises a worldwide group of non-calcified or calcified, crust-forming red algae found in diverse, intertidal to deep subtidal marine habitats. Eight genera have been recognized in the family, with Peyssonnelia Decaisne having the largest number of species. Both comparative morphology and rbcL and nuclear LSU rDNA sequence data support the monophyly of the family and show that it cannot be maintained in the order Gigartinales Schmitz. A new order, Peyssonneliales, is herein proposed to accommodate the Peysonneliaceae, with only two of the genera (i.e., Peyssonnelia and Sonderopelta), and its relationship to the other red algal orders is discussed. We also propose the transfer of one species, Peyssonnelia capensis Montagne to Sonderopelta Womersley & Sinkora.
C1 [Norris, James N.] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Krayesky, David M.; Gabriel, Daniela; Fredericq, Suzanne] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA.
[Gabrielson, Paul W.] Univ N Carolina, Herbarium, Chapel Hill, NC 27599 USA.
RP Norris, JN (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM david.krayesky@sru.edu; norrisj@si.edu; drseaweed@hotmail.com;
danielagabriel@gmail.com; slf9209@louisiana.edu
RI Gabriel, Daniela/L-7869-2013
OI Gabriel, Daniela/0000-0002-0362-6274
FU NSF [DEB-0328491, DEB-0919508, DEB-0315995, DEB-0743024]; US-Panama
Cooperative Research Program [OISE-0819205]
FX We thank all collectors listed in Table 2, and the RN-Pelican (LUMCON)
crew for their help in collecting subtidal, crustose algae. Our
appreciation goes to numerous colleagues who have offered comments and
discussions that have lead to improvement of our manuscript. This study
was supported by NSF Systematic Biology: PEET (DEB-0328491), and
Peyssonneliaceae (DEB-0919508); NSF Biodiversity Inventories: Gulf of
Mexico (DEB-0315995, and Panama (DEB-0743024); US-Panama Cooperative
Research Program (OISE-0819205). This research represents Smithsonian
Marine Station at Fort Pierce Contribution No. SMSFP-791, and Caribbean
Coral Reef Ecosystem Program of the National Museum of Natural History
Contribution No. CCRE-862.
NR 109
TC 20
Z9 21
U1 0
U2 3
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD OCT 14
PY 2009
VL 122
IS 3
BP 364
EP 391
PG 28
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 511EB
UT WOS:000271145600010
ER
PT J
AU Groot, PJ
Verbeek, K
Greimel, R
Irwin, M
Gonzalez-Solares, E
Gansicke, BT
de Groot, E
Drew, J
Augusteijn, T
Aungwerojwit, A
Barlow, M
Barros, S
van den Besselaar, EJM
Casares, J
Corradi, R
Corral-Santana, JM
Deacon, N
van Ham, W
Hu, HL
Heber, U
Jonker, PG
King, R
Knigge, C
Mampaso, A
Marsh, TR
Morales-Rueda, L
Napiwotzki, R
Naylor, T
Nelemans, G
Oosting, T
Pyrzas, S
Pretorius, M
Rodriguez-Gil, P
Roelofs, GHA
Sale, S
Schellart, P
Steeghs, D
Szyszka, C
Unruh, Y
Walton, NA
Weston, S
Witham, A
Woudt, P
Zijlstra, A
AF Groot, Paul J.
Verbeek, Kars
Greimel, Robert
Irwin, Mike
Gonzalez-Solares, Eduardo
Gaensicke, Boris T.
de Groot, Eelco
Drew, Janet
Augusteijn, Thomas
Aungwerojwit, Amornrat
Barlow, Mike
Barros, Susana
van den Besselaar, Else J. M.
Casares, Jorge
Corradi, Romano
Corral-Santana, Jesus M.
Deacon, Niall
van Ham, Wilbert
Hu, Haili
Heber, Uli
Jonker, Peter G.
King, Rob
Knigge, Christian
Mampaso, Antonio
Marsh, Tom R.
Morales-Rueda, Luisa
Napiwotzki, Ralf
Naylor, Tim
Nelemans, Gijs
Oosting, Tim
Pyrzas, Stylianos
Pretorius, Magaretha
Rodriguez-Gil, Pablo
Roelofs, Gijs H. A.
Sale, Stuart
Schellart, Pim
Steeghs, Danny
Szyszka, Cezary
Unruh, Yvonne
Walton, Nicholas A.
Weston, Simon
Witham, Andrew
Woudt, Patrick
Zijlstra, Albert
TI The UV-Excess survey of the northern Galactic plane
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; stars: general; ISM: general; Galaxy: disc; Galaxy: stellar
content; Galaxy: structure
ID DIGITAL SKY SURVEY; AM-CVN STARS; H-ALPHA SURVEY; CATACLYSMIC VARIABLES;
PROPER MOTIONS; BRIGHT STARS; WHITE-DWARFS; FINDING LIST; DATA RELEASE;
X-RAY
AB The UV-Excess survey of the northern Galactic plane images a 10 degrees x 185 degrees wide band, centred on the Galactic equator using the 2.5-m Isaac Newton Telescope in four bands (U, g, r, He 15875) down to similar to 21-22 mag (similar to 20 in He 15875). The setup and data reduction procedures are described. Simulations of the colours of main-sequence stars, giant, supergiants, DA and DB white dwarfs and AM Canum Venaticorum stars are made, including the effects of reddening. A first look at the data of the survey (currently 30 per cent complete) is given.
C1 [Groot, Paul J.; Verbeek, Kars; de Groot, Eelco; van den Besselaar, Else J. M.; Deacon, Niall; van Ham, Wilbert; Hu, Haili; Morales-Rueda, Luisa; Nelemans, Gijs; Oosting, Tim; Schellart, Pim] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Greimel, Robert; Corradi, Romano; Pyrzas, Stylianos; Rodriguez-Gil, Pablo] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain.
[Greimel, Robert] Karl Franzen Univ Graz, Inst Phys, A-8010 Graz, Austria.
[Irwin, Mike; Gonzalez-Solares, Eduardo; Walton, Nicholas A.] Univ Cambridge, Inst Astron, Cambridge Astron Survey Unit, Cambridge CB3 0HA, England.
[Gaensicke, Boris T.; Aungwerojwit, Amornrat; Barros, Susana; Marsh, Tom R.; Pyrzas, Stylianos; Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Drew, Janet; Napiwotzki, Ralf; Weston, Simon] Univ Hertfordshire, Ctr Astron Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Augusteijn, Thomas] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Canary Islands, Spain.
[Aungwerojwit, Amornrat] Naresuan Univ, Dept Phys, Fac Sci, Phitsanulok 65000, Thailand.
[Barlow, Mike] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Casares, Jorge; Corradi, Romano; Corral-Santana, Jesus M.; Mampaso, Antonio; Rodriguez-Gil, Pablo] Inst Astrofis Canarias, E-38208 Tenerife, Spain.
[Heber, Uli] Univ Erlangen Nurnberg, D-96049 Bamberg, Germany.
[Jonker, Peter G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, Peter G.; Roelofs, Gijs H. A.; Steeghs, Danny] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[King, Rob; Naylor, Tim] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Knigge, Christian; Witham, Andrew] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Pretorius, Magaretha] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Sale, Stuart; Unruh, Yvonne] Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Szyszka, Cezary] European So Observ, D-85748 Garching, Germany.
[Woudt, Patrick] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa.
[Zijlstra, Albert] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
RP Groot, PJ (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM pgroot@astro.ru.nl
RI Sale, Stuart/E-1815-2010; Gaensicke, Boris/A-9421-2012; Barlow,
Michael/A-5638-2009; Naylor, Tim /A-9465-2015; Corral-Santana,
Jesus/A-6956-2016; Groot, Paul/K-4391-2016; Rodriguez-Gil,
Pablo/H-7709-2015; Nelemans, Gijs/D-3177-2012; Steeghs,
Danny/C-5468-2009; Heber, Ulrich/G-3306-2013
OI Barros, Susana/0000-0003-2434-3625; Drew, Janet/0000-0003-1192-7082;
Gaensicke, Boris/0000-0002-2761-3005; Barlow,
Michael/0000-0002-3875-1171; Corral-Santana, Jesus/0000-0003-1038-9104;
Groot, Paul/0000-0002-4488-726X; Rodriguez-Gil,
Pablo/0000-0002-4717-5102; Unruh, Yvonne/0000-0001-8217-6998; Sale,
Stuart/0000-0003-2155-0995; Nelemans, Gijs/0000-0002-0752-2974; Steeghs,
Danny/0000-0003-0771-4746; Heber, Ulrich/0000-0001-7798-6769
NR 46
TC 33
Z9 33
U1 0
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 11
PY 2009
VL 399
IS 1
BP 323
EP 339
DI 10.1111/j.1365-2966.2009.15273.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 511KN
UT WOS:000271163200027
ER
PT J
AU Soleri, P
Tudose, V
Fender, R
van der Klis, M
Jonker, PG
AF Soleri, Paolo
Tudose, Valeriu
Fender, Rob
van der Klis, Michiel
Jonker, Peter G.
TI Linking jet emission and X-ray properties in the peculiar neutron star
X-ray binary Circinus X-1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: Cir X-1; stars: neutron;
ISM: jets and outflows; X-rays: binaries
ID QUASI-PERIODIC OSCILLATIONS; TIMING-EXPLORER OBSERVATIONS; BLACK-HOLE
CANDIDATE; LARGE-SCALE JET; LOW-FREQUENCY; RADIO OBSERVATIONS; SPECTRAL
BEHAVIOR; SCORPIUS X-1; CYGNUS X-2; CIR X-1
AB We present the results of simultaneous X-ray and radio observations of the peculiar Z-type neutron star X-ray binary Cir X-1, observed with the Rossi X-ray Timing Explorer satellite and the Australia Telescope Compact Array in 2000 October and 2002 December. We identify typical Z-source behaviour in the power density spectra as well as characteristic Z patterns drawn in an X-ray hardness-intensity diagram. Power spectra typical of bright atoll sources have also been identified at orbital phases after the periastron passage, while orbital phases before the periastron passage are characterized by power spectra that are typical neither of Z nor of atoll Sources. We investigate the coupling between the X-ray and the radio properties, focusing oil three orbital phases when an enhancement of the radio flux density has been detected, to test the link between the inflow (X-ray) and the Outflow (radio jet) to/from the compact object. In two out of three cases, we associate the presence of the radio jet to a spectral transition in the X-rays, although the transition does not precede the radio flare, as detected in other Z sources. An analogous behaviour has recently been found in the black hole candidate GX 339-4. In the third case, the radio light curve shows a similar shape to the X-ray light curve. We discuss our results in the context of jet models, considering also black hole candidates.
C1 [Soleri, Paolo; Tudose, Valeriu; Fender, Rob; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Tudose, Valeriu] Acad Romana, Astron Inst, RO-040557 Bucharest, Romania.
[Tudose, Valeriu] Res Ctr Atom Phys & Astrophys, RO-077125 Bucharest, Romania.
[Tudose, Valeriu] Netherlands Inst Radio Astron, NL-7991 PD Dwingeloo, Netherlands.
[Fender, Rob] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Jonker, Peter G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Jonker, Peter G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Soleri, P (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
EM p.soleri@uva.nl
RI Tudose, Valeriu/F-8976-2010
FU Netherlands Organization for Scientific Research (NWO); Australian
Commonwealth Scientific and Research Organization (CSIRO)
FX PS acknowledges Support from a Netherlands Organization for Scientific
Research (NWO) VIDI awarded to RF and a NWO Spinoza awarded to MVDK. The
Australia Telescope is funded by the Commonwealth of Australia for
operations as a national facility managed by the Australian Commonwealth
Scientific and Research Organization (CSIRO). This research has made use
of data obtained through the High Energy Astrophysics Science Archive
Research Centel Online Service, provided by the NASA Goddard space
flight center.
NR 77
TC 13
Z9 13
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 11
PY 2009
VL 399
IS 1
BP 453
EP 464
DI 10.1111/j.1365-2966.2009.15297.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 511KN
UT WOS:000271163200039
ER
PT J
AU Chan, CK
AF Chan, Chi-kwan
TI OSCILLATIONS OF THE INNER REGIONS OF VISCOUS ACCRETION DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; hydrodynamics; instabilities; waves
ID DIFFERENTIALLY ROTATING-DISKS; QUASI-PERIODIC OSCILLATIONS; NONLINEAR
CONSERVATION-LAWS; SPECTRAL VISCOSITY METHOD; BLACK-HOLES; RESONANT
EXCITATION; DYNAMICAL STABILITY; TIME VARIABILITY; SIMULATED DISKS;
NEUTRON-STARS
AB Although quasi-periodic oscillations (QPOs) have been discovered in different X-ray sources, their origin is still a matter of debate. Analytical studies of hydrodynamic accretion disks have shown three types of trapped global modes with properties that appear to agree with the observations. However, these studies take only the linear effects into account. Moreover, observations suggest that resonances between modes play a crucial role. A systematic, numerical study of this problem is therefore needed. In this paper, we use a pseudo-spectral algorithm to perform a parameter study of the inner regions of hydrodynamic disks. By assuming a-viscosity, we show that steady state solutions rarely exist. The inner edges of the disks oscillate and excite axisymmetric waves, which provide a plausible explanation for the high-frequency QPOs observed from accreting black holes. In addition, the flows inside the inner edges are sometimes unstable to non-axisymmetric perturbations. One-armed, or even two-armed, spirals are developed. When the Reynolds numbers are above certain critical values, the inner disks go through some transient turbulent states characterized by strong trailing spirals; while large-scale leading spirals are developed in the outer disks. We compared our numerical results with standard thin disk oscillation models. Albeit the non-axisymmetric features have their analytical counterparts, more careful study is needed to explain the axisymmetric oscillations.
C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
EM ckchan@cfa.harvard.edu
FU ITC fellowship
FX The author thanks Ramesh Narayan, Alexander Tchekhovskoy, Ruth
Murray-Clay, and Robert Penna for useful discussions; Dimitrios Psaltis,
Feryal Ozel, Martin Pessah, and Sukanya Chakrabarti for giving detailed
comments on the manuscript; Gordon Ogilvie for pointing out important
references on hydrodynamic overstability; Ken Henisey and Omer Blaes for
kindly sharing their ongoing work on disk oscillations. The simulations
presented in this paper were performed on a Beowulf cluster in the
Physics Department at University of Arizona. The author is currently
supported by an ITC fellowship.
NR 52
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 68
EP 79
DI 10.1088/0004-637X/704/1/68
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500006
ER
PT J
AU Cotton, WD
Ragland, S
Pluzhnik, E
Danchi, WC
Traub, WA
Willson, LA
Lacasse, MG
AF Cotton, W. D.
Ragland, S.
Pluzhnik, E.
Danchi, W. C.
Traub, W. A.
Willson, L. A.
Lacasse, M. G.
TI SIO MASERS IN ASYMMETRIC MIRAS. I. R LEONIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio lines: stars; stars: AGB and post-AGB; stars: atmospheres
ID LATE-TYPE STARS; VARIABLE-STARS; VLBA OBSERVATIONS; SHELL
AB This is the first paper in a series of multi-epoch observations of the SiO masers at 7 mm wavelength in several asymptotic giant branch (AGB) stars. This is a sample of Mira variable stars showing evidence of asymmetric structure in the infrared which were observed interferometrically in the infrared by Infrared Optical Telescope Array and with Very Long Baseline Array measurements of the SiO masers. In this paper, we present the observations of R Leonis (R Leo). During the period of observations, this star shows extended emission with large-scale coherent patterns in the radial velocity, possibly the result of ejecting a substantial amount of material, largely to the west. This is interpreted as an event in which material is expelled in a collimated flow, possibly following an energetic event. If common, these events may help explain the asymmetric nature of the planetary nebulae that develop from AGB stars. The systemic velocity of R Leo is estimated to be +1.0 +/- 0.3 km s(-1). All observed radial velocities are well below the escape velocity.
C1 [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ragland, S.; Pluzhnik, E.] Calif Assoc Res Astron, Kamuela, HI 96743 USA.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Willson, L. A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA.
[Lacasse, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
EM bcotton@nrao.edu
FU NSF [AST-0456047]
FX We acknowledge support from NSF through grant AST-0456047.
NR 13
TC 5
Z9 5
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 170
EP 182
DI 10.1088/0004-637X/704/1/170
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500015
ER
PT J
AU Roman-Zuniga, CG
Lada, CJ
Alves, JF
AF Roman-Zuniga, Carlos G.
Lada, Charles J.
Alves, Joao F.
TI HIGH RESOLUTION NEAR-INFRARED SURVEY OF THE PIPE NEBULA. I. A DEEP
INFRARED EXTINCTION MAP OF BARNARD 59
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: globules; stars: formation
ID MASSIVE STAR-FORMATION; DENSE CORE POPULATION; MOLECULAR CLOUDS;
DARK-CLOUD; INTERSTELLAR EXTINCTION; IC 5146; FRAGMENTATION; FIELD;
DUST; LAW
AB We present our analysis of a fully sampled, high resolution dust extinction map of the Barnard 59 complex in the Pipe Nebula. The map was constructed with the infrared color excess technique applied to a photometric catalog that combines data from both ground and space based observations. The map resolves for the first time the high density center of the main core in the complex, which is associated with the formation of a small cluster of stars. We found that the central core in Barnard 59 shows an unexpected lack of significant substructure consisting of only two significant fragments. Overall, the material appears to be consistent with being a single, large core with a density profile that can be well fit by a King model. A series of NH(3) pointed observations toward the high column density center of the core appear to show that the core is still thermally dominated, with subsonic non-thermal motions. The stars in the cluster could be providing feedback to support the core against collapse, but the relatively narrow radio lines suggest that an additional source of support, for example, amagnetic field, may be required to stabilize the core. Outside the central core our observations reveal the structure of peripheral cores and resolve an extended filament into a handful of significant substructures whose spacing and masses appear to be consistent with Jeans fragmentation.
C1 [Roman-Zuniga, Carlos G.; Alves, Joao F.] Ctr Astron Hispano Aleman, Granada 18006, Spain.
[Roman-Zuniga, Carlos G.; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02143 USA.
[Roman-Zuniga, Carlos G.; Alves, Joao F.] Inst Astrofis Andalucia, Granada 18006, Spain.
RP Roman-Zuniga, CG (reprint author), Ctr Astron Hispano Aleman, Granada 18006, Spain.
RI Roman-Zuniga, Carlos/F-6602-2016;
OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Alves,
Joao/0000-0002-4355-0921
FU NASA [NAG 13041, GO20119]; JPL [1279166]
FX We thank Jill Rathborne for providing the reduction and model fit of the
NH3 data as part of a GBT survey of dense cores in the Pipe
Nebula. We thank August Muench, Kevin Covey, Doug Johnstone, and Paula
Teixeira for useful discussions and suggestions. This project
acknowledges support from NASA Origins Program (NAG 13041), NASA Spitzer
Program GO20119, and JPL contract 1279166. This work is based in part on
observations made with ESO Telescopes at the La Silla and Paranal
Observatories under programs 069.C-0426 and 071.C-0324. This work is
based in part on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. This publication makes use of
data products from the Two Micron All Sky Survey, which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation.
NR 51
TC 21
Z9 21
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 183
EP 195
DI 10.1088/0004-637X/704/1/183
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500016
ER
PT J
AU Forbrich, J
Lada, CJ
Muench, AA
Alves, J
Lombardi, M
AF Forbrich, Jan
Lada, Charles J.
Muench, August A.
Alves, Joao
Lombardi, Marco
TI A SPITZER CENSUS OF STAR FORMATION ACTIVITY IN THE PIPE NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; stars: formation; stars: pre-main sequence
ID SPECTRAL ENERGY-DISTRIBUTIONS; NEARBY DENSE CORES; YOUNG STELLAR
OBJECTS; T-TAURI STARS; C2D SURVEY; MOLECULAR CLOUDS; MASS FUNCTION;
LUMINOSITIES; POPULATION; DISCOVERY
AB The Pipe Nebula, a large nearby molecular cloud, lacks obvious signposts of star formation in all but one of more than 130 dust extinction cores that have been identified within it. In order to quantitatively determine the current level of star formation activity in the Pipe Nebula, we analyzed 13 deg(2) of sensitive mid-infrared maps of the entire cloud, obtained with the Multiband Imaging Photometer for Spitzer at wavelengths of 24 mu m and 70 mu m, to search for candidate young stellar objects (YSOs) in the high-extinction regions. We argue that our search is complete for class I and typical class II YSOs with luminosities of L(bol) similar to 0.2 L(circle dot) and greater. We find only 18 candidate YSOs in the high-extinction regions of the entire Pipe cloud. Twelve of these sources are previously known members of a small cluster associated with Barnard 59, the largest and most massive dense core in the cloud. With only six candidate class I and class II YSOs detected toward extinction cores outside of this cluster, our findings emphatically confirm the notion of an extremely low level of star formation activity in the Pipe Nebula. The resulting star formation efficiency for the entire cloud mass is only similar to 0.06%.
C1 [Forbrich, Jan; Lada, Charles J.; Muench, August A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Alves, Joao] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain.
[Lombardi, Marco] European So Observ, D-85748 Garching, Germany.
RP Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jforbrich@cfa.harvard.edu; clada@cfa.harvard.edu;
amuench@cfa.harvard.edu; jalves@caha.es; mlombard@eso.org
OI Muench, August/0000-0003-0666-6367; LOMBARDI, MARCO/0000-0002-3336-4965;
Alves, Joao/0000-0002-4355-0921
FU NASA [1279166]; National Science Foundation
FX We thank Thomas Robitaille for help with the SED fits. This work is
based on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. Support for this work was
provided by NASA through an award issued by JPL/Caltech, contract
1279166. This publication makes use of data products from the Two Micron
All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation.
NR 32
TC 31
Z9 31
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 292
EP 305
DI 10.1088/0004-637X/704/1/292
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500025
ER
PT J
AU Su, YN
van Ballegooijen, A
Schmieder, B
Berlicki, A
Guo, Y
Golub, L
Huang, GL
AF Su, Yingna
van Ballegooijen, Adriaan
Schmieder, Brigitte
Berlicki, Arkadiusz
Guo, Yang
Golub, Leon
Huang, Guangli
TI FLARE ENERGY BUILD-UP IN A DECAYING ACTIVE REGION NEAR A CORONAL HOLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments; Sun: flares; Sun: magnetic fields; Sun:
photosphere; Sun: X-rays, gamma rays
ID RAY TELESCOPE XRT; MAGNETIC-FIELDS; FORCE-FREE; MASS EJECTIONS;
SOLAR-FLARES; RECONNECTION; FILAMENT; FLUX; THEMIS; MODEL
AB A B1.7 two-ribbon flare occurred in a highly non-potential decaying active region near a coronal hole at 10: 00 UT on 2008 May 17. This flare is "large" in the sense that it involves the entire region, and it is associated with both a filament eruption and a coronal mass ejection. We present multi-wavelength observations from EUV (TRACE, STEREO/EUVI), X-rays (Hinode/XRT), and Ha (THEMIS, BBSO) prior to, during and after the flare. Prior to the flare, the region contained two filaments. The long J-shaped sheared loops corresponding to the southern filament were evolved from two short loop systems, which happened around 22: 00 UT after a filament eruption on May 16. Formation of highly sheared loops in the southeastern part of the region was observed by STEREO 8 hr before the flare. We also perform nonlinear force-free field (NLFFF) modeling for the region at two times prior to the flare, using the flux rope insertion method. The models include the non-force-free effect of magnetic buoyancy in the photosphere. The best-fit NLFFF models show good fit to observations both in the corona (X-ray and EUV loops) and chromosphere (Ha filament). We find that the horizontal fields in the photosphere are relatively insensitive to the present of flux ropes in the corona. The axial flux of the flux rope in the NLFFF model on May 17 is twice that on May 16, and the model on May 17 is only marginally stable. We also find that the quasi-circular flare ribbons are associated with the separatrix between open and closed fields. This observation and NLFFF modeling suggest that this flare may be triggered by the reconnection at the null point on the separatrix surface.
C1 [Su, Yingna; van Ballegooijen, Adriaan; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Su, Yingna; Huang, Guangli] Purple Mt Observ, Nanjing 210008, Peoples R China.
[Schmieder, Brigitte; Berlicki, Arkadiusz; Guo, Yang] LESIA, Sect Meudon, Observ Paris, F-92195 Meudon, France.
[Berlicki, Arkadiusz] ASCR, Astron Inst, Ondrejov 25165, Czech Republic.
[Berlicki, Arkadiusz] Univ Wroclaw, Astron Inst, PL-51140 Wroclaw, Poland.
RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM ynsu@head.cfa.harvard.edu
RI Guo, Yang/A-9134-2012; Su, Yingna/J-1674-2012; Berlicki,
Arkadiusz/G-9001-2014;
OI Guo, Yang/0000-0002-9293-8439; van Ballegooijen,
Adriaan/0000-0002-5622-3540; Golub, Leon/0000-0001-9638-3082
NR 56
TC 31
Z9 31
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 OCT 10
PY 2009
VL 704
IS 1
BP 341
EP 353
DI 10.1088/0004-637X/704/1/341
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500028
ER
PT J
AU Torok, T
Aulanier, G
Schmieder, B
Reeves, KK
Golub, L
AF Torok, T.
Aulanier, G.
Schmieder, B.
Reeves, K. K.
Golub, L.
TI FAN-SPINE TOPOLOGY FORMATION THROUGH TWO-STEP RECONNECTION DRIVEN BY
TWISTED FLUX EMERGENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; MHD; Sun: corona; Sun: magnetic fields
ID CORONAL MASS EJECTIONS; X-RAY JETS; DYNAMIC MAGNETIC RECONNECTION;
QUASI-SEPARATRIX LAYERS; SOLAR-FLARES; EMERGING FLUX; ALFVEN WAVES;
NULL-POINT; HINODE; MODEL
AB We address the formation of three-dimensional nullpoint topologies in the solar corona by combining Hinode/X-ray Telescope (XRT) observations of a small dynamic limb event, which occurred beside a non-erupting prominence cavity, with a three-dimensional (3D) zero-beta magnetohydrodynamics (MHD) simulation. To this end, we model the boundary-driven "kinematic" emergence of a compact, intense, and uniformly twisted flux tube into a potential field arcade that overlies a weakly twisted coronal flux rope. The expansion of the emerging flux in the corona gives rise to the formation of a nullpoint at the interface of the emerging and the pre-existing fields. We unveil a two-step reconnection process at the nullpoint that eventually yields the formation of a broad 3D fan-spine configuration above the emerging bipole. The first reconnection involves emerging fields and a set of large-scale arcade field lines. It results in the launch of a torsional MHD wave that propagates along the arcades, and in the formation of a sheared loop system on one side of the emerging flux. The second reconnection occurs between these newly formed loops and remote arcade fields, and yields the formation of a second loop system on the opposite side of the emerging flux. The two loop systems collectively display an anenome pattern that is located below the fan surface. The flux that surrounds the inner spine field line of the nullpoint retains a fraction of the emerged twist, while the remaining twist is evacuated along the reconnected arcades. The nature and timing of the features which occur in the simulation do qualititatively reproduce those observed by XRT in the particular event studied in this paper. Moreover, the two-step reconnection process suggests a new consistent and generic model for the formation of anemone regions in the solar corona.
C1 [Torok, T.; Aulanier, G.; Schmieder, B.] Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92190 Meudon, France.
[Reeves, K. K.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Torok, T (reprint author), Univ Paris Diderot, Univ Paris 06, CNRS, Observ Paris,LESIA, 5 Pl Jules Janssen, F-92190 Meudon, France.
RI Reeves, Katharine/P-9163-2014
FU European Commission [MTRN-CT-2006-035484, 218816]
FX We thank the referee for detailed comments and suggestions which helped
very much to improve the quality of this paper. Financial support by the
European Commission through the SOLAIRE Network (MTRN-CT-2006-035484)
and through the FP7 SOTERIA project (Grant Agreement no. 218816) are
gratefully acknowledged.
NR 58
TC 71
Z9 71
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 485
EP 495
DI 10.1088/0004-637X/704/1/485
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500037
ER
PT J
AU Brown, JM
Blake, GA
Qi, C
Dullemond, CP
Wilner, DJ
Williams, JP
AF Brown, J. M.
Blake, G. A.
Qi, C.
Dullemond, C. P.
Wilner, D. J.
Williams, J. P.
TI EVIDENCE FOR DUST CLEARING THROUGH RESOLVED SUBMILLIMETER IMAGING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems: protoplanetary disks; stars: pre-main sequence
ID MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; PROTOPLANETARY DISK
GAPS; INTERMEDIATE-MASS STARS; HERBIG AE STARS; T-TAURI STARS;
CIRCUMSTELLAR DISKS; YOUNG STARS; GM AURIGAE; INNER HOLE
AB Mid-infrared spectrophotometric observations have revealed a small subclass of circumstellar disks with spectral energy distributions (SEDs) suggestive of large inner gaps with low dust content. However, such data provide only an indirect and model-dependent method of finding central holes. Imaging of protoplanetry disks provides an independent check of SED modeling. We present here the direct characterization of three 33-47 AU radii inner gaps, in the disks around LkH alpha 330, SR 21N, and HD 135344B, via 340 GHz (880 mu m) dust continuum aperture synthesis observations obtained with the Submillimeter Array (SMA). The large gaps are fully resolved at similar to 0 ''.3 by the SMA data and mostly empty of dust, with less than (1-7.5) x 10(-6) M-circle dot of fine grained solids inside the holes. Gas (as traced by atomic accretion markers and CO 4.7 mu m rovibrational emission) is still present in the inner regions of all three disks. For each, the inner hole exhibits a relatively steep rise in dust emission to the outer disk, a feature more likely to originate from the gravitational influence of a companion body than from a process expected to show a more shallow gradient like grain growth. Importantly, the good agreement between the spatially resolved data and spectrophotometry-based models lends confidence to current interpretations of SEDs, wherein the significant dust emission deficits arise from disks with inner gaps or holes. Further SED-based searches can therefore be expected to yield numerous additional candidates that can be examined at high spatial resolution.
C1 [Brown, J. M.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
[Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Qi, C.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dullemond, C. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Williams, J. P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Brown, JM (reprint author), Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
EM jbrown@mpe.mpg.de
OI Williams, Jonathan/0000-0001-5058-695X; Dullemond,
Cornelis/0000-0002-7078-5910
FU Smithsonian Institution; Academia Sinica
FX The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Acadenia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica.
NR 47
TC 136
Z9 136
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 496
EP 502
DI 10.1088/0004-637X/704/1/496
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500038
ER
PT J
AU Giannini, T
Lorenzetti, D
Elia, D
Strafella, F
De Luca, M
Fazio, G
Marengo, M
Nisini, B
Smith, HA
AF Giannini, T.
Lorenzetti, D.
Elia, D.
Strafella, F.
De Luca, M.
Fazio, G.
Marengo, M.
Nisini, B.
Smith, H. A.
TI PRE-MAIN SEQUENCE VARIABLES IN THE VMR-D: IDENTIFICATION OF T TAURI-LIKE
ACCRETING PROTOSTARS THROUGH SPITZER-IRAC VARIABILITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; infrared: ISM; infrared: stars; stars: formation; stars:
pre-main sequence; stars: variables: other
ID VELA MOLECULAR CLOUDS; YOUNG STELLAR OBJECTS; STAR-FORMATION; C2D
SURVEY; INTERSTELLAR CLOUDS; SPACE-TELESCOPE; EXOR VARIABLES; EMBEDDED
STAR; SERPENS; NEARBY
AB We present a study of the infrared variability of young stellar objects by means of two Spitzer-IRAC images of the Vela Molecular Cloud D (VMR-D) obtained in observations separated in time by about six months. By using the same space-born IR instrumentation, this study eliminates all the unwanted effects due to differences in sensitivity, confusion, saturation, calibration, and filter bandpasses, issues that are usually unavoidable when comparing catalogs obtained from different instruments. The VMR-D map covers about 1.5 deg(2) of a site where star formation is actively ongoing. We are interested in accreting pre-main sequence variables whose luminosity variations are due to intermittent events of disk accretion (i.e., active T Tauri stars and EXor-type objects). The variable objects have been selected from a catalog of more than 170,000 sources detected at an S/N >= 5. We then searched the sample of variables for ones whose photometric properties such as IR excess, color-magnitude relationships, and spectral energy distribution, are as close as possible to those of known EXor's. Indeed, the latter are monitored in a more systematic way than T Tauri stars and the mechanisms that regulate the observed phenomenology are exactly the same. Hence, themodalities of the EXor behavior are adopted as driving criterion for selecting variables in general. We ultimately selected 19 bona fide candidates that constitute a well defined sample of new variable targets for further investigation (monitoring, spectroscopy). Out of these, 10 sources present a Spitzer MIPS 24 mu m counterpart, and have been classified as three Class I, five flat spectrum, and two Class II objects, while the spectral energy distribution of the other nine sources is compatible with evolutionary phases older than Class I. This is consistent with what is known about the small sample of known EXor's, whose properties have driven the present selection and suggests that the accretion flaring or EXor stage might come as a ClassI/ClassII transition. We also present new prescriptions that can be useful in future searches for accretion variables in large IR databases.
C1 [Giannini, T.; Lorenzetti, D.; De Luca, M.; Nisini, B.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Elia, D.] Univ Lisbon, Fac Ciencias, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal.
[Elia, D.; Strafella, F.] Univ Salento, Dipartimento Fis, I-73100 Lecce, Italy.
[De Luca, M.] Observ Paris, CNRS, UMR 8112, LERMA LRA, F-75231 Paris, France.
[De Luca, M.] Ecole Normale Super, F-75231 Paris, France.
[Fazio, G.; Marengo, M.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Giannini, T (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
EM giannini@oa-roma.inaf.it; dloren@oa-roma.inaf.it; eliad@oal.ul.pt;
francesco.strafella@le.infn.it; deluca@oa-roma.inaf.it;
mmarengo@cfa.harvard.edu; nisini@oa-roma.inaf.it; hsmith@cfa.harvard.edu
OI Lorenzetti, Dario/0000-0001-6415-4162; Elia, Davide/0000-0002-9120-5890;
Giannini, Teresa/0000-0002-0224-096X; , Brunella
Nisini/0000-0002-9190-0113
FU NASA [1256790]
FX The authors thank Arkady A. Arkharov andValeri M. Larionov for providing
them with the near IR spectra of the sources win35 and win70, taken at
Campo Imperatore (Italy). This work is based on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under NASA contract 1407.
Support for the IRAC instrument was provided by NASA under contract
number 1256790 issued by JPL.
NR 45
TC 9
Z9 9
U1 1
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 OCT 10
PY 2009
VL 704
IS 1
BP 606
EP 617
DI 10.1088/0004-637X/704/1/606
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500047
ER
PT J
AU Mandel, KS
Wood-Vasey, WM
Friedman, AS
Kirshner, RP
AF Mandel, Kaisey S.
Wood-Vasey, W. Michael
Friedman, Andrew S.
Kirshner, Robert P.
TI TYPE Ia SUPERNOVA LIGHT-CURVE INFERENCE: HIERARCHICAL BAYESIAN ANALYSIS
IN THE NEAR-INFRARED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE distance scale; supernovae: general
ID HUBBLE-SPACE-TELESCOPE; DARK ENERGY; ACCELERATING UNIVERSE; CEPHEID
CALIBRATIONS; DISTANCE INDICATORS; PRECISE DISTANCE; CROSS-VALIDATION;
HIGH-REDSHIFT; KEY PROJECT; CONSTANT
AB We present a comprehensive statistical analysis of the properties of Type Ia supernova (SN Ia) light curves in the near-infrared using recent data from Peters Automated InfraRed Imaging TELescope and the literature. We construct a hierarchical Bayesian framework, incorporating several uncertainties including photometric error, peculiar velocities, dust extinction, and intrinsic variations, for principled and coherent statistical inference. SN Ia light-curve inferences are drawn from the global posterior probability of parameters describing both individual supernovae and the population conditioned on the entire SN Ia NIR data set. The logical structure of the hierarchical model is represented by a directed acyclic graph. Fully Bayesian analysis of the model and data is enabled by an efficient Markov Chain Monte Carlo algorithm exploiting the conditional probabilistic structure using Gibbs sampling. We apply this framework to the JHKs SN Ia light-curve data. A new light-curve model captures the observed J-band light-curve shape variations. The marginal intrinsic variances in peak absolute magnitudes are sigma(M-J) = 0.17+/-0.03, sigma(M-H) = 0.11+/-0.03, and sigma(M-Ks) = 0.19+/-0.04. We describe the first quantitative evidence for correlations between the NIR absolute magnitudes and J-band light-curve shapes, and demonstrate their utility for distance estimation. The average residual in the Hubble diagram for the training set SNe at cz > 2000 km s(-1) is 0.10 mag. The new application of bootstrap cross-validation to SN Ia light-curve inference tests the sensitivity of the statistical model fit to the finite sample and estimates the prediction error at 0.15 mag. These results demonstrate that SN Ia NIR light curves are as effective as corrected optical light curves, and, because they are less vulnerable to dust absorption, they have great potential as precise and accurate cosmological distance indicators.
C1 [Mandel, Kaisey S.; Wood-Vasey, W. Michael; Friedman, Andrew S.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Mandel, KS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM kmandel@cfa.harvard.edu
RI Friedman, Andrew/I-4691-2013
OI Friedman, Andrew/0000-0003-1334-039X
FU NSF [AST06-06772, AST-057475]; Harvard University Milton Fund;
University of Virginia; SAO; UC Berkeley; National Aeronautics and Space
Administration (NASA [NNG06GH50G]
FX Supernova research at Harvard University is supported by NSF grant
AST06-06772. The Peters Automated InfraRed Imaging TELescope (PAIRITEL)
is operated by the Smithsonian Astrophysical Observatory (SAO) and was
made possible by a grant from the Harvard University Milton Fund, the
camera loan from the University of Virginia, and the continued support
of the SAO and UC Berkeley. Partial support for PAIRITEL operations
comes from National Aeronautics and Space Administration (NASA) grant
NNG06GH50G ("PAIRITEL: Infrared Followup for Swift Transients"). This
publication makes use of data products from the 2MASS, funded by NASA
and the US National Science Foundation (NSF). IAUC/CBET were useful. M.
W. V. is funded by a grant from the US National Science Foundation
(AST-057475). A. S. F. acknowledges support from an NSF Graduate
Research Fellowship and a NASA Graduate Research Program Fellowship.
NR 81
TC 55
Z9 57
U1 1
U2 6
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 OCT 10
PY 2009
VL 704
IS 1
BP 629
EP 651
DI 10.1088/0004-637X/704/1/629
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500049
ER
PT J
AU Miller-Ricci, E
Meyer, MR
Seager, S
Elkins-Tanton, L
AF Miller-Ricci, Eliza
Meyer, Michael R.
Seager, Sara
Elkins-Tanton, Linda
TI ON THE EMERGENT SPECTRA OF HOT PROTOPLANET COLLISION AFTERGLOWS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems
ID TERRESTRIAL PLANET FORMATION; EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS;
SUPER-EARTHS; KEPLER MISSION; GIANT PLANETS; HARPS SEARCH; MASS; VENUS;
SYSTEM
AB We explore the appearance of terrestrial planets in formation by studying the emergent spectra of hot molten protoplanets during their collisional formation. While such collisions are rare, the surfaces of these bodies may remain hot at temperatures of 1000-3000 K for up to millions of years during the epoch of their formation (of duration 10-100 Myr). These objects are luminous enough in the thermal infrared to be observable with current and next-generation optical/IR telescopes, provided that the atmosphere of the forming planet permits astronomers to observe brightness temperatures approaching that of the molten surface. Detectability of a collisional afterglow depends on properties of the planet's atmosphere-primarily on the mass of the atmosphere. A planet with a thin atmosphere is more readily detected, because there is little atmosphere to obscure the hot surface. Paradoxically, a more massive atmosphere prevents one from easily seeing the hot surface, but also keeps the planet hot for a longer time. In terms of planetary mass, more massive planets are also easier to detect than smaller ones because of their larger emitting surface areas-up to a factor of 10 in brightness between 1 and 10 M(circle plus) planets. We present preliminary calculations assuming a range of protoplanet masses (1-10 M(circle plus)), surface pressures (1-1000 bar), and atmospheric compositions, for molten planets with surface temperatures ranging from 1000 to 1800 K, in order to explore the diversity of emergent spectra that are detectable. While current 8 to 10 m class ground-based telescopes may detect hot protoplanets at wide orbital separations beyond 30 AU (if they exist), we will likely have to wait for next-generation extremely large telescopes or improved diffraction suppression techniques to find terrestrial planets in formation within several AU of their host stars.
C1 [Miller-Ricci, Eliza] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Meyer, Michael R.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA.
RP Miller-Ricci, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM emillerricci@cfa.harvard.edu
RI Elkins-Tanton, Linda/C-5508-2008
OI Elkins-Tanton, Linda/0000-0003-4008-1098
FU Harvard Origins of Life Initiative; Smithsonian Astrophysical
Observatory; NASA [NNG06GH25G]; NSF
FX We thank Bruce Macintosh for sharing his insight on exoplanet imaging
techniques and Dan Fabricant for discussions of the imaging capabilities
of the GMT. We also thank Phil Hinz, ScottKenyon, and Eric Mamajek for
useful discussions. M. R. M. acknowledges the Harvard Origins of Life
Initiative, the Smithsonian Astrophysical Observatory, and a NASA TPF
Foundation Science Program grant NNG06GH25G (PI: S. Kenyon) for
sabbatical support. L. E.-T. acknowledges funding from the NSF astronomy
program.
NR 57
TC 11
Z9 11
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 770
EP 780
DI 10.1088/0004-637X/704/1/770
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500060
ER
PT J
AU Younger, JD
Fazio, GG
Huang, JS
Yun, MS
Wilson, GW
Ashby, MLN
Gurwell, MA
Peck, AB
Petitpas, GR
Wilner, DJ
Hughes, DH
Aretxaga, I
Kim, S
Scott, KS
Austermann, J
Perera, T
Lowenthal, JD
AF Younger, Joshua D.
Fazio, Giovanni G.
Huang, Jia-Sheng
Yun, Min S.
Wilson, Grant W.
Ashby, Matthew L. N.
Gurwell, Mark A.
Peck, Alison B.
Petitpas, Glen R.
Wilner, David J.
Hughes, David H.
Aretxaga, Itziar
Kim, Sungeun
Scott, Kimberly S.
Austermann, Jason
Perera, Thushara
Lowenthal, James D.
TI THE AzTEC/SMA INTERFEROMETRIC IMAGING SURVEY OF SUBMILLIMETER-SELECTED
HIGH-REDSHIFT GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: high-redshift; galaxies: starburst; submillimeter
ID HUBBLE-DEEP-FIELD; BACKGROUND EXPERIMENT SEARCH; ULTRALUMINOUS INFRARED
GALAXIES; DEGREE EXTRAGALACTIC SURVEY; SUPERMASSIVE BLACK-HOLES;
SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; SPECTRAL
ENERGY-DISTRIBUTION; PHASE CALIBRATION SOURCES; EVOLUTION SURVEY COSMOS
AB We present results from a continuing interferometric survey of high-redshift submillimeter galaxies (SMGs) with the Submillimeter Array, including high-resolution (beam size similar to 2 arcsec) imaging of eight additional AzTEC 1.1 mm selected sources in the COSMOS field, for which we obtain six reliable (peak signal-to-noise ratio (S/N) > 5 or peak S/N > 4 with multiwavelength counterparts within the beam) and two moderate significance (peak S/N > 4) detections. When combined with previous detections, this yields an unbiased sample of millimeter-selected SMGs with complete interferometric follow up. With this sample in hand, we (1) empirically confirm the radio-submillimeter association, (2) examine the submillimeter morphology-including the nature of SMGs with multiple radio counterparts and constraints on the physical scale of the far infrared-of the sample, and (3) find additional evidence for a population of extremely luminous, radio-dim SMGs that peaks at higher redshift than previous, radio-selected samples. In particular, the presence of such a population of high-redshift sources has important consequences for models of galaxy formation-which struggle to account for such objects even under liberal assumptions-and dust production models given the limited time since the big bang.
C1 [Younger, Joshua D.; Fazio, Giovanni G.; Huang, Jia-Sheng; Ashby, Matthew L. N.; Gurwell, Mark A.; Petitpas, Glen R.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Yun, Min S.; Wilson, Grant W.; Scott, Kimberly S.; Austermann, Jason; Perera, Thushara] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Peck, Alison B.] Joint ALMA Off, Santiago 7550108, Chile.
[Hughes, David H.; Aretxaga, Itziar] INAOE, Tonantzintla, Peubla, Mexico.
[Kim, Sungeun] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea.
[Lowenthal, James D.] Smith Coll, Dept Astron, Clark Sci Ctr, Northampton, MA 01060 USA.
RP Younger, JD (reprint author), Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA.
EM jyounger@ias.edu
FU Smithsonian Institution; Academia Sinica; NASA [1407, HF-51266.01, NAS
5-26555]; NSF [0540852]; Korea Science and Engineering Foundation
(KOSEF); CONACyT
FX We thank the referee for their comments, and Lars Hernquist, Doug
Finkbeiner, John Huchra, and Dave Sanders for helpful discussions. The
Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica. This work is based on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under NASA contact 1407.
This work is partially funded by NSF Grant 0540852. The JCMT/AzTEC
Survey and S. K. were supported in part by the Korea Science and
Engineering Foundation (KOSEF) under a cooperative agreement with the
Astrophysical Research Center of the Structure and Evolution of the
Cosmos (ARCSEC). J. D. Y. acknowledges support from NASA through Hubble
Fellowship grant HF-51266.01 awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. D. H.
H. and I. A. are supported in part by CONACyT.
NR 146
TC 63
Z9 63
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 803
EP 812
DI 10.1088/0004-637X/704/1/803
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500063
ER
PT J
AU Schmelz, JT
Kashyap, VL
Saar, SH
Dennis, BR
Grigis, PC
Lin, L
DeLuca, EE
Holman, GD
Golub, L
Weber, MA
AF Schmelz, J. T.
Kashyap, V. L.
Saar, S. H.
Dennis, B. R.
Grigis, P. C.
Lin, L.
DeLuca, E. E.
Holman, G. D.
Golub, L.
Weber, M. A.
TI SOME LIKE IT HOT: CORONAL HEATING OBSERVATIONS FROM HINODE X-RAY
TELESCOPE AND RHESSI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: X-rays, gamma rays
ID SOLAR ACTIVE REGIONS; ATOMIC DATABASE; EMISSION-LINES; ABUNDANCES;
RECONSTRUCTION; SPECTRA; MISSION; CHIANTI; PLASMA; SHEETS
AB We have used Hinode X-Ray Telescope observations and RHESSI upper limits together to characterize the differential emission measure (DEM) from a quiescent active region. We find a relatively smooth DEM curve with the expected active region peak at log T = 6.4. We also find a high-temperature component with significant emission measure at log T greater than or similar to 7. This curve is consistent with previous observations of quiescent active regions in that it does not produce observable Fe XIX lines. It is different from that generated with X-Ray Telescope (XRT) data alone-RHESSI rules out the possibility of a separate high-temperature component with a peak of approximately log T = 7.4. The strength and position of the high-temperature peak in this XRT-only analysis was, however, poorly determined; adding RHESSI flux upper limits in the 4-13 keV energy range provide a strong high-temperature constraint which greatly improves the multi-thermal findings. The results of the present work as well as those from a growing number of papers on this subject imply that our previous understanding of the temperature distribution in active regions has been limited. Hot plasma (log T approximate to 7) appears to be prevalent, although in relatively small quantities as predicted by nanoflare models. Other models may need to be adjusted or updated to account for these new results.
C1 [Schmelz, J. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Schmelz, J. T.; Kashyap, V. L.; Saar, S. H.; Grigis, P. C.; DeLuca, E. E.; Golub, L.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dennis, B. R.; Holman, G. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lin, L.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012; DeLuca,
Edward/L-7534-2013
OI DeLuca, Edward/0000-0001-7416-2895
FU NASA [NNG05GM44G, NAS8-39073]; NSF [ATM-0402729]
FX We thank Piet Martens, Fabio Reale, and Jim Klimchuk for helpful
discussions. Richard Schwartz measured the RHESSI background data used
here to compute upper limits and provided the instrument response.
Hinode is a Japanese mission developed and launched by ISAS/JAXA, with
NAOJ as domestic partner and NASA and STFC (UK) as international
partners. It is operated by these agencies in co-operation with ESA and
the NSC (Norway). Solar physics research at the University of Memphis is
supported by a Hinode subcontract from NASA/SAO as well as NSF
ATM-0402729. V. K. acknowledges support from NASA-LWSTRT Grant
NNG05GM44G and NASA contract NAS8-39073 to the Chandra X-ray Center.
NR 26
TC 31
Z9 31
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 863
EP 869
DI 10.1088/0004-637X/704/1/863
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500067
ER
PT J
AU Berger, E
Cenko, SB
Fox, DB
Cucchiara, A
AF Berger, E.
Cenko, S. B.
Fox, D. B.
Cucchiara, A.
TI DISCOVERY OF THE VERY RED NEAR-INFRARED AND OPTICAL AFTERGLOW OF THE
SHORT-DURATION GRB 070724A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: bursts
ID GAMMA-RAY BURST; HOST GALAXY; CONSTRAINTS; GRB-060121; GRB-050709;
REDSHIFT; EMISSION
AB We report the discovery of the near-infrared and optical afterglow of the short-duration gamma-ray burst GRB 070724A. The afterglow is detected in iJHK(s) observations starting 2.3 hr after the burst with K(s) = 19.59 +/- 0.16 mag and i = 23.79 +/- 0.07 mag, but is absent in images obtained 1.3 yr later. Fading is also detected in the K(s) band between 2.8 and 3.7 hr at a 4 sigma significance level. The optical/near-IR spectral index, beta(O), (NIR) approximate to -2, is much redder than expected in the standard afterglow model, pointing to either significant dust extinction, A(V)(host) approximate to 2 mag, or a non-afterglow origin for the near-IR emission. The case for extinction is supported by a shallow optical to X-ray spectral index, consistent with the definition for "dark bursts," and a normal near-IR to X-ray spectral index. Moreover, a comparison to the optical discovery magnitudes of all short GRBs with optical afterglows indicates that the near-IR counterpart of GRB 070724A is one of the brightest to date, while its observed optical emission is one of the faintest. In the context of a non-afterglow origin, the near-IR emission may be dominated by a mini-supernova (mini-SN), leading to an estimated ejected mass of M similar to 10(-4) M(circle dot) and a radioactive energy release efficiency of f similar to 5 x 10(-3) (for v similar to 0.3c). However, the mini-SN model predicts a spectral peak in the UV rather than near-IR, suggesting that this is either not the correct interpretation or that the mini-SN models need to be revised. Finally, the afterglow coincides with a star-forming galaxy at z = 0.457, previously identified as the host based on its coincidence with the X-ray afterglow position (similar to 2 '' radius). Our discovery of the optical/near-IR afterglow makes this association secure, and furthermore localizes the burst to the outskirts of the galaxy, with an offset of 4.8 +/- 0.1 kpc relative to the host center. At such a large offset, the possible large extinction points to a dusty environment local to the burst and rules out a halo or intergalactic origin.
C1 [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fox, D. B.; Cucchiara, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 37
TC 22
Z9 24
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2009
VL 704
IS 1
BP 877
EP 882
DI 10.1088/0004-637X/704/1/877
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KR
UT WOS:000270219500069
ER
PT J
AU Giacintucci, S
Venturi, T
Cassano, R
Dallacasa, D
Brunetti, G
AF Giacintucci, S.
Venturi, T.
Cassano, R.
Dallacasa, D.
Brunetti, G.
TI A GIANT RADIO HALO IN THE MASSIVE AND MERGING CLUSTER ABELL 1351
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; galaxies: clusters: individual (A 1351);
radiation mechanisms: non-thermal; radio continuum: general; X-rays:
general
ID GALAXY CLUSTERS; REACCELERATION; EMISSION; CONSTRAINTS; STATISTICS;
SAMPLE; ORIGIN; MODEL; COMA
AB We report on the detection of diffuse radio emission in the X-ray luminous and massive galaxy cluster A 1351 (z = 0.322) using archival Very Large Array data at 1.4 GHz. Given its central location, morphology, and Mpc-scale extent, we classify the diffuse source as a giant radio halo. X-ray and weak lensing studies show A 1351 to be a system undergoing a major merger. The halo is associated with the most massive substructure. The presence of this source is explained assuming that merger-driven turbulence may re-accelerate high-energy particles in the intracluster medium and generate diffuse radio emission on the cluster scale. The position of A 1351 in the log P(1.4GHz)-log L(X) plane is consistent with that of all other radio-halo clusters known to date, supporting a causal connection between the unrelaxed dynamical state of massive (> 10(15) M(circle dot)) clusters and the presence of giant radio halos.
C1 [Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Giacintucci, S.; Venturi, T.; Cassano, R.; Dallacasa, D.; Brunetti, G.] INAF IRA, I-40129 Bologna, Italy.
[Cassano, R.; Dallacasa, D.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy.
RP Giacintucci, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Cassano, Rossella/0000-0003-4046-0637; Brunetti,
Gianfranco/0000-0003-4195-8613; Venturi, Tiziana/0000-0002-8476-6307
FU INAF [PRIN-INAF2007, PRIN-INAF2008]; ASI-INAF [I/088/06/0]
FX This work is partially supported by INAF under grants PRIN-INAF2007 and
PRIN-INAF2008 and by ASI-INAF under grant I/088/06/0.
NR 21
TC 12
Z9 12
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2009
VL 704
IS 1
BP L54
EP L57
DI 10.1088/0004-637X/704/1/L54
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KT
UT WOS:000270219700012
ER
PT J
AU Muzerolle, J
Flaherty, K
Balog, Z
Furlan, E
Smith, PS
Allen, L
Calvet, N
D'Alessio, P
Megeath, ST
Muench, A
Rieke, GH
Sherry, WH
AF Muzerolle, James
Flaherty, Kevin
Balog, Zoltan
Furlan, Elise
Smith, Paul S.
Allen, Lori
Calvet, Nuria
D'Alessio, Paola
Megeath, S. Thomas
Muench, August
Rieke, George H.
Sherry, William H.
TI EVIDENCE FOR DYNAMICAL CHANGES IN A TRANSITIONAL PROTOPLANETARY DISK
WITH MID-INFRARED VARIABILITY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; planetary systems: protoplanetary disks;
stars: pre-main sequence
ID PRE-MAIN-SEQUENCE; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS;
MULTIBAND IMAGING PHOTOMETER; ALL-SKY SURVEY; MASS STARS; INFRARED
SPECTROGRAPH; INTERSTELLAR CLOUDS; MOLECULAR CLOUD; C2D SURVEY
AB We present multi-epoch Spitzer Space Telescope observations of the transitional disk LRLL 31 in the 2-3 Myr old star-forming region IC 348. Our measurements show remarkable mid-infrared variability on timescales as short as one week. The infrared continuum emission exhibits systematic wavelength-dependent changes that suggest corresponding dynamical changes in the inner disk structure and variable shadowing of outer disk material. We propose several possible sources for the structural changes, including a variable accretion rate or a stellar or planetary companion embedded in the disk. Our results indicate that variability studies in the infrared can provide important new constraints on protoplanetary disk behavior.
C1 [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Muzerolle, James; Flaherty, Kevin; Balog, Zoltan; Smith, Paul S.; Rieke, George H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Balog, Zoltan] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Furlan, Elise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Allen, Lori; Muench, August] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofis, Morelia, Michoacan, Mexico.
[Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Sherry, William H.] Natl Solar Observ, Tucson, AZ 85719 USA.
RP Muzerolle, J (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
OI Muench, August/0000-0003-0666-6367; Furlan, Elise/0000-0001-9800-6248
FU NASA [1407, 960785]
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 NASA contract 1407. Support for
this work was provided by NASA through Contract Number 960785 issued by
JPL/Caltech. We acknowledge K. Luhman for assistance with spectral
typing the SpeX spectrum.
NR 37
TC 52
Z9 52
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2009
VL 704
IS 1
BP L15
EP L19
DI 10.1088/0004-637X/704/1/L15
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KT
UT WOS:000270219700004
ER
PT J
AU Reale, F
McTiernan, JM
Testa, P
AF Reale, Fabio
McTiernan, James M.
Testa, Paola
TI COMPARISON OF HINODE/XRT AND RHESSI DETECTION OF HOT PLASMA IN THE
NON-FLARING SOLAR CORONA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: X-rays, gamma rays
ID X-RAY; ACTIVE REGIONS; TELESCOPE; EMISSION; MISSION
AB We compare observations of the non-flaring solar corona made simultaneously with Hinode/XRT and RHESSI. The analyzed corona is dominated by a single active region on 2006 November 12. The comparison is made on emission measures. We derive emission measure distributions versus temperature of the entire active region from multifilter XRT data. We check the compatibility with the total emission measure values estimated from the flux measured with RHESSI if the emission comes from isothermal plasma. We find that RHESSI and XRT data analyses consistently point to the presence of a minor emission measure component peaking at log T similar to 6.8-6.9. The discrepancy between XRT and RHESSI results is within a factor of a few and indicates an acceptable level of cross-consistency.
C1 [Reale, Fabio] Univ Palermo, Dipartimento Sci Fisiche & Astron, Sez Astron, I-90134 Palermo, Italy.
[McTiernan, James M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reale, Fabio] Osservatorio Astron Palermo GS Vaiana, INAF, I-90134 Palermo, Italy.
RP Reale, F (reprint author), Univ Palermo, Dipartimento Sci Fisiche & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy.
OI Reale, Fabio/0000-0002-1820-4824
FU Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale
Italiana [I/015/07/0, I/023/09/0]; NASA [NNM07AA02C, NAS5-98033,
NNX08AJ18G]
FX We thank H. Hudson for triggering this work, and J. Klimchuk and the
anonymous referee for comments and suggestions. Hinode is a Japanese
mission developed and launched by ISAS/JAXA, with NAOJ as domestic
partner and NASA and STFC (UK) as international partners. It is operated
by these agencies in cooperation with ESA and NSC ( Norway). F. R.
acknowledges support from Italian Ministero dell'Universita e Ricerca
and Agenzia Spaziale Italiana (ASI), contracts I/015/07/0 and
I/023/09/0. P. T. is supported by NASA contract NNM07AA02C to SAO. J. M.
is supported by NASA contract NAS5-98033 and NASA grant NNX08AJ18G.
NR 12
TC 22
Z9 22
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2009
VL 704
IS 1
BP L58
EP L61
DI 10.1088/0004-637X/704/1/L58
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KT
UT WOS:000270219700013
ER
PT J
AU Zapata, LA
Schmid-Burgk, J
Ho, PTP
Rodriguez, LF
Menten, KM
AF Zapata, Luis A.
Schmid-Burgk, Johannes
Ho, Paul T. P.
Rodriguez, Luis F.
Menten, Karl M.
TI EXPLOSIVE DISINTEGRATION OF A MASSIVE YOUNG STELLAR SYSTEM IN ORION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual (Orion BN/KL); ISM: jets and outflows; ISM: molecules;
ISM: Herbig-Haro objects; radio lines: ISM; techniques: interferometric
ID PROPER MOTIONS; BN OBJECT; NEBULA; REGION; STAR; OUTFLOW; RESOLUTION;
FEATURES; ARRAY; SOUTH
AB Young massive stars in the center of crowded star clusters are expected to undergo close dynamical encounters that could lead to energetic, explosive events. However, there has so far never been clear observational evidence of such a remarkable phenomenon. We here report new interferometric observations that indicate the well-known enigmatic wide-angle outflow located in the Orion BN/KL star-forming region to have been produced by such a violent explosion during the disruption of a massive young stellar system, and that this was caused by a close dynamical interaction about 500 years ago. This outflow thus belongs to a totally different family of molecular flows that is not related to the classical bipolar flows that are generated by stars during their formation process. Our molecular data allow us to create a three-dimensional view of the debris flow and to link this directly to the well-known Orion H(2) "fingers" farther out.
C1 [Zapata, Luis A.; Schmid-Burgk, Johannes; Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rodriguez, Luis F.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
RP Zapata, LA (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
NR 24
TC 56
Z9 57
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2009
VL 704
IS 1
BP L45
EP L48
DI 10.1088/0004-637X/704/1/L45
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 499KT
UT WOS:000270219700010
ER
PT J
AU Zhang, P
Kharchenko, V
Dalgarno, A
Matsumi, Y
Nakayama, T
Takahashi, K
AF Zhang, P.
Kharchenko, V.
Dalgarno, A.
Matsumi, Y.
Nakayama, T.
Takahashi, K.
TI Comment on "Approach to Thermal Equilibrium in Atomic Collisions" Reply
SO PHYSICAL REVIEW LETTERS
LA English
DT Editorial Material
ID ELECTRON THERMALIZATION; GASES; HE
C1 [Zhang, P.; Kharchenko, V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Matsumi, Y.; Nakayama, T.; Takahashi, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Matsumi, Y.; Nakayama, T.; Takahashi, K.] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648601, Japan.
RP Zhang, P (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RI Nakayama, Tomoki/I-6230-2014
OI Nakayama, Tomoki/0000-0002-5554-1272
NR 7
TC 2
Z9 2
U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD OCT 9
PY 2009
VL 103
IS 15
AR 159302
DI 10.1103/PhysRevLett.103.159302
PG 1
WC Physics, Multidisciplinary
SC Physics
GA 505EK
UT WOS:000270672100059
ER
PT J
AU Jiang, L
Hodges, JS
Maze, JR
Maurer, P
Taylor, JM
Cory, DG
Hemmer, PR
Walsworth, RL
Yacoby, A
Zibrov, AS
Lukin, MD
AF Jiang, L.
Hodges, J. S.
Maze, J. R.
Maurer, P.
Taylor, J. M.
Cory, D. G.
Hemmer, P. R.
Walsworth, R. L.
Yacoby, A.
Zibrov, A. S.
Lukin, M. D.
TI Repetitive Readout of a Single Electronic Spin via Quantum Logic with
Nuclear Spin Ancillae
SO SCIENCE
LA English
DT Article
ID DIAMOND; ENTANGLEMENT; ALGORITHMS; DYNAMICS; QUBITS
AB Robust measurement of single quantum bits plays a key role in the realization of quantum computation and communication as well as in quantum metrology and sensing. We have implemented a method for the improved readout of single electronic spin qubits in solid-state systems. The method makes use of quantum logic operations on a system consisting of a single electronic spin and several proximal nuclear spin ancillae in order to repetitively readout the state of the electronic spin. Using coherent manipulation of a single nitrogen vacancy center in room-temperature diamond, full quantum control of an electronic-nuclear system consisting of up to three spins was achieved. We took advantage of a single nuclear-spin memory in order to obtain a 10-fold enhancement in the signal amplitude of the electronic spin readout. We also present a two-level, concatenated procedure to improve the readout by use of a pair of nuclear spin ancillae, an important step toward the realization of robust quantum information processors using electronic-and nuclear-spin qubits. Our technique can be used to improve the sensitivity and speed of spin-based nanoscale diamond magnetometers.
C1 [Jiang, L.; Hodges, J. S.; Maze, J. R.; Maurer, P.; Walsworth, R. L.; Yacoby, A.; Zibrov, A. S.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Hodges, J. S.; Cory, D. G.] MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA.
[Taylor, J. M.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Hemmer, P. R.] Texas A&M Univ, Dept Elect & Comp Engn, College Stn, TX 77843 USA.
[Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lukin, MD (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
EM lukin@fas.harvard.edu
RI Hodges, Jonathan/G-1034-2010; Taylor, Jacob/B-7826-2011; Zibrov,
Alexander/G-7419-2014; Jiang, Liang/A-9847-2008;
OI Taylor, Jacob/0000-0003-0493-5594; Jiang, Liang/0000-0002-0000-9342;
Hodges, Jonathan/0000-0002-3487-6698
FU Defense Advanced Research Projects Agency; NSF; Packard Foundation;
Pappalardo Fellowship
FX We thank P. Cappellaro, L. Childress, J. Doyle, M. V. G. Dutt, J.
MacArthur, A. Sorenson, P. Stanwix, E. Togan, and A. Trifonov for many
stimulating discussions and experimental help. This work was supported
by the Defense Advanced Research Projects Agency, NSF, the Packard
Foundation, and the Pappalardo Fellowship. The content of the
information does not necessarily reflect the position or the policy of
the U.S. Government, and no official endorsement should be inferred.
NR 31
TC 144
Z9 144
U1 3
U2 48
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD OCT 9
PY 2009
VL 326
IS 5950
BP 267
EP 272
DI 10.1126/science.1176496
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 504EX
UT WOS:000270599500037
PM 19745117
ER
PT J
AU Blank, SM
Taeger, A
Liston, AD
Smith, DR
Rasnitsyn, AP
Shinohara, A
Heidemaa, M
Viitasaari, M
AF Blank, Stephan M.
Taeger, Andreas
Liston, Andrew D.
Smith, David R.
Rasnitsyn, Alexandr P.
Shinohara, Akihiko
Heidemaa, Mikk
Viitasaari, Matti
TI Studies toward a World Catalog of Symphyta (Hymenoptera)
SO ZOOTAXA
LA English
DT Review
DE Sawflies; nomenclature; taxonomy; bibliography; new species; new
synonymy; new combination; lectotype; neotype; type species designation
ID GENUS PHYLLOCOLPA; GROUP INSECTA; TENTHREDINIDAE; NEMATINAE; PART;
PHYLOGENY; SAWFLIES; REGION; MONGOLIA; REVISION
AB Taxonomic and nomenclatorial changes affecting Symphyta, resulting from work on a forthcoming world catalog, are proposed and explained. Dolerus zhelochovtsevi Heidemaa & Viitasaari, sp. nov. is described. One former subgenus and two former subspecies are now treated at genus or species level, respectively. Eighteen replacement names are given, 73 new synonymies and 78 new combinations are proposed, 3 synonymies are re-established, and 5 names are resurrected from synonymy. The precedence of 18 species names (nomina protecta) over their older synonyms (20 nomina oblita) is explained. Type species are designated for 8 genus-group names. One neotype and 17 lectotypes are designated. Five names described as varieties are assigned infrasubspecific rank. Twenty-five genus-group names associated with Arge, Corynis, Dolerus, Trichiosoma and Xyela are unavailable. Two genus-group names and 33 species-group names are considered as unplaced taxa. An identification key is presented for the West Palaearctic species of Profenusa MacGillivray, 1914. Notes on publication dates and authorships of names of certain taxa are also included.
C1 [Blank, Stephan M.; Taeger, Andreas; Liston, Andrew D.] Senckenberg Deutsch Entomol Inst, D-15374 Muncheberg, Germany.
[Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Rasnitsyn, Alexandr P.] Russian Acad Sci, Palaeontol Inst, Moscow 117997, Russia.
[Rasnitsyn, Alexandr P.] Nat Hist Museum, London SW7 5BD, England.
[Shinohara, Akihiko] Natl Museum Nat & Sci, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan.
[Heidemaa, Mikk] Univ Tartu, Inst Ecol & Earth Sci, Dept Zool, EE-51014 Tartu, Estonia.
[Viitasaari, Matti] Univ Helsinki, Dept Appl Biol, FIN-00014 Helsinki, Finland.
RP Blank, SM (reprint author), Senckenberg Deutsch Entomol Inst, Eberswalder Str 90, D-15374 Muncheberg, Germany.
EM stephan.blank@senckenberg.de; andreas.taeger@senckenberg.de;
andrew.liston@senckenberg.de; dave.smith@ars.usda.gov;
rasna36@yahoo.com; shinohar@kahaku.go.jp; mikk.heidemaa@ut.ee;
matti.viitasaari@netsonic.fi
FU European Commission's (FP 6) [DK-TAF 4845 / SE-TAF 4856]; Federal
Ministry for Education and Research [BMBF] of Germany; Global
Biodiversity information Facility [GBIF], Copenhagen; Estonian Science
Foundation [6598]; Estonian Ministry of Education and Science
[SF0180122s08]
FX We cordially thank the following colleagues for their support: Jean-Yves
Baugnee (Gembloux) and Jean-Luc Boeve (Brussels) for the larval record
of Dolerus zhelochovtsevi from Belgium; Sergey Belokobylskij (St.
Petersburg) for searching for original material of Andre, Eversmann,
Gussakovskij and Jakowlew in the ZIN collection; Gavin Broad (London)
for photographs of the very rare work by Donovan (1808); Rainer Emmrich
(Dresden) for information on the proper publication date of Profenusa
aspoecki; Toshiya Hirowatari (Sakai) and Masaaki Suwa (Sapporo) for
allowing examination of Arge captiva material in their respective
collections; Seppo Hornytzkyi and Simo Lehtinen (Mikrofokus Ltd,
Helsinki) for enabling access to their SEM; Frank Koch (Berlin) for
checking the ZMHB for specimens labelled by Klug as Brachytomus or
Brachytoma; Kazuhiko Konishi (Sapporo) for providing a copy of Uchiyama
(1906); Manfred Kraus (Nurnberg) for supplying information on Diprion
pini; Christian Kutzscher (Muncheberg) for translations from Swedish
publications; Andre Nel (Paris) for discussing with us the Proximoxeris
problem; James P. O'Connor (Dublin) for his information regarding the
type material of Gmelin; Ene-Reet Soovik and Janika Pall (Tartu) for
translations from Latin and Swedish; Mare Toom (Tartu) for the
identification of the host plant of Dolerus zhelochovtsevi; Sergey
Vasilenko (Novosibirsk) for clarification of publication details for
Arge zhelochovzevi; Lars Vilhelmsen (Copenhagen) for translating Danish
texts and searching for material in the ZMUC collection. A number of
additional colleagues listed under Material & Methods have made their
collections accessible for us or have mailed material on loan. Holger
Framke, Ute Kaczinski and Renate Riedelsheimer of the DEI library
(Muncheberg) have never tired in trying to satisfy our seemingly
insatiable requests for rare and obscure publications about Symphyta.
Manuscripts on Hemichroa and Hylotoma, which earlier were intended as
applications to the International Commission on Zoological Nomenclature,
were critically checked by dagger I. M. Kerzhner (St. Petersburg),
dagger H. Pschorn-Walcher (Neulengbach), W. Schedl (Innsbruck), and A.
Zinovjev (Boston / St. Petersburg). Gary Gibson (Ottawa), Henri Goulet
(Ottawa) and Veli Vikberg (Turenki) reviewed the manuscript within a
remarkably short time and sent us many helpful comments. S. M. Blank's
work at the Natural History Museum of Denmark in Copenhagen and A.
Taeger's work at the Swedish Museum of Natural History was supported by
grants from the European Commission's (FP 6) Integrated Infrastructure
Initiative programme SYNTHESYS (DK-TAF 4845 / SE-TAF 4856).
Contributions of A. D. Liston, A. Taeger and S. M Blank partly result
from the project "GISHym: Global Information System on Hymenoptera"
(GBIF-D, Global Biodiversity Information Facility Initiative of Germany
funded by the Federal Ministry for Education and Research [BMBF] of
Germany) and from the project "ECatSym: Electronic World Catalog of
Symphyta (Hymenoptera)" (funded by the Global Biodiversity information
Facility [GBIF], Copenhagen). M. Heidemaa was financially supported by
the Estonian Science Foundation (grant number 6598), the Estonian
Ministry of Education and Science (target-financing project number
SF0180122s08) and the European Union through the European Regional
Development Fund (Center of Excellence FIBIR).
NR 441
TC 14
Z9 20
U1 1
U2 4
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD OCT 8
PY 2009
IS 2254
BP 1
EP 96
PG 96
WC Zoology
SC Zoology
GA 503UJ
UT WOS:000270565800001
ER
PT J
AU Kingston, SE
Adams, LD
Rosel, PE
AF Kingston, Sarah E.
Adams, Lara D.
Rosel, Patricia E.
TI Testing mitochondrial sequences and anonymous nuclear markers for
phylogeny reconstruction in a rapidly radiating group: molecular
systematics of the Delphininae (Cetacea: Odontoceti: Delphinidae)
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Review
ID FRAGMENT LENGTH POLYMORPHISM; MULTILOCUS GENOTYPE DATA; GULF-OF-MEXICO;
SP N. CETACEA; POPULATION-STRUCTURE; CYTOCHROME-B; GENETIC
DIFFERENTIATION; DOLPHINS GENUS; LAKE MALAWI; SYMPATRIC MORPHOTYPES
AB Background: Many molecular phylogenetic analyses rely on DNA sequence data obtained from single or multiple loci, particularly mitochondrial DNA loci. However, phylogenies for taxa that have undergone recent, rapid radiation events often remain unresolved. Alternative methodologies for discerning evolutionary relationships under these conditions are desirable. The dolphin subfamily Delphininae is a group that has likely resulted from a recent and rapid radiation. Despite several efforts, the evolutionary relationships among the species in the subfamily remain unclear.
Results: Here, we compare a phylogeny estimated using mitochondrial DNA (mtDNA) control region sequences to a multi-locus phylogeny inferred from 418 polymorphic genomic markers obtained from amplified fragment length polymorphism (AFLP) analysis. The two sets of phylogenies are largely incongruent, primarily because the mtDNA tree provides very poor resolving power; very few species' nodes in the tree are supported by bootstrap resampling. The AFLP phylogeny is considerably better resolved and more congruent with relationships inferred from morphological data. Both phylogenies support paraphyly for the genera Stenella and Tursiops. The AFLP data indicate a close relationship between the two spotted dolphin species and recent ancestry between Stenella clymene and S. longirostris. The placement of the Lagenodelphis hosei lineage is ambiguous: phenetic analysis of the AFLP data is consistent with morphological expectations but the phylogenetic analysis is not.
Conclusion: For closely related, recently diverged taxa, a multi-locus genome-wide survey is likely the most comprehensive approach currently available for phylogenetic inference.
C1 [Kingston, Sarah E.; Adams, Lara D.; Rosel, Patricia E.] NOAA Fisheries, SE Fisheries Sci Ctr, Lafayette, LA 70506 USA.
[Kingston, Sarah E.] Univ Maryland, Coll Chem & Life Sci, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA.
[Kingston, Sarah E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA.
[Adams, Lara D.] Natl Ocean Serv, Charleston, SC 29412 USA.
RP Rosel, PE (reprint author), NOAA Fisheries, SE Fisheries Sci Ctr, 646 Cajundome Blvd,Suite 234, Lafayette, LA 70506 USA.
EM kingstons@si.edu; Lara.Adams@noaa.gov; Patricia.Rosel@noaa.gov
NR 118
TC 31
Z9 33
U1 1
U2 18
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD OCT 7
PY 2009
VL 9
AR 245
DI 10.1186/1471-2148-9-245
PG 19
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 520ZK
UT WOS:000271888200001
PM 19811651
ER
PT J
AU Angelier, F
Holberton, RL
Marra, PP
AF Angelier, Frederic
Holberton, Rebecca L.
Marra, Peter P.
TI Does stress response predict return rate in a migratory bird species? A
study of American redstarts and their non-breeding habitat
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE corticosterone; survival; stress; environmental context; habitat
ID NONBREEDING SEASON; CORTICOSTERONE RESPONSES; INDIVIDUAL VARIATION; FOOD
AVAILABILITY; CLIFF SWALLOWS; HORMONE-LEVELS; REPRODUCTION; SELECTION;
BEHAVIOR; QUALITY
AB In vertebrates, the adrenocortical stress response activates an emergency life-history stage, which is thought to promote survival by helping individuals escape life-threatening situations. Although the adrenocortical stress response promotes many behavioural and physiological changes, it remains unclear whether this stress response actually translates into higher survival in wild vertebrates. We measured the adrenocortical stress response of non-breeding American redstarts (Setophaga ruticilla), a migratory bird that wintered in habitats of either high (mangroves) or low suitability (scrubs), and subsequently monitored their return rate during the following non-breeding seasons. The intensity of the adrenocortical stress response was consistent within individuals across the non-breeding season and was positively correlated with return rates in redstarts that wintered in scrubs, but not in redstarts that wintered in mangroves. Thus, in a context-dependent manner, the ability of an individual to physiologically react to stress determines its ability of returning to its non-breeding territory the following winters. For an individual, the ability to mount an important adrenocortical stress response probably benefits to survival. However, this beneficial effect probably depends on an individual's environment and phenotypic characteristics because these two variables are likely to affect its probability of being confronted with life-threatening stressors during its annual life cycle.
C1 [Angelier, Frederic; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[Holberton, Rebecca L.] Univ Maine, Lab Avian Biol, Sch Biol & Ecol, Orono, ME 04469 USA.
RP Angelier, F (reprint author), Univ Calif Davis, Dept Neurobiol Physiol & Behav, 1 Shields Ave, Davis, CA 95616 USA.
EM fangelier@ucdavis.edu
FU NSF [0649679, 0717338]
FX This study was supported by an NSF grant (0649679) to P. P. M. and R. L.
H. and an NSF grant (0717338) to P. P. M. We thank M. Dawkins, O.
Chastel, C. M. Vleck, D. Vleck, M. Palacios, M. Shultz and two anonymous
reviewers, who gave very helpful comments on a previous version of the
manuscript. We thank the Petroleum Corporation of Jamaica for permission
to conduct this research at the Font Hill Nature Preserve, and Yvette
Strong and Andrea Donaldson of the Jamaica National Environmental
Planning Agency for their cooperation.
NR 51
TC 48
Z9 48
U1 1
U2 31
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P R SOC B
JI Proc. R. Soc. B-Biol. Sci.
PD OCT 7
PY 2009
VL 276
IS 1672
BP 3545
EP 3551
DI 10.1098/rspb.2009.0868
PG 7
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 486ZZ
UT WOS:000269241300019
PM 19605397
ER
PT J
AU Lerner, HRL
Johnson, JA
Lindsay, AR
Kiff, LF
Mindell, DP
AF Lerner, Heather R. L.
Johnson, Jeff A.
Lindsay, Alec R.
Kiff, Lloyd F.
Mindell, David P.
TI It's not too Late for the Harpy Eagle (Harpia harpyja): High Levels Of
Genetic Diversity and Differentiation Can Fuel Conservation Programs
SO PLOS ONE
LA English
DT Article
AB Background: The harpy eagle (Harpia harpyja) is the largest Neotropical bird of prey and is threatened by human persecution and habitat loss and fragmentation. Current conservation strategies include local education, captive rearing and reintroduction, and protection or creation of trans-national habitat blocks and corridors. Baseline genetic data prior to reintroduction of captive-bred stock is essential for guiding such efforts but has not been gathered previously.
Methodology/Findings: We assessed levels of genetic diversity, population structure and demographic history for harpy eagles using samples collected throughout a large portion of their geographic distribution in Central America (n = 32) and South America (n = 31). Based on 417 bp of mitochondrial control region sequence data, relatively high levels of haplotype and nucleotide diversity were estimated for both Central and South America, although haplotype diversity was significantly higher for South America. Historical restriction of gene flow across the Andes (i.e. between our Central and South American subgroups) is supported by coalescent analyses, the haplotype network and significant F(ST) values, however reciprocally monophyletic lineages do not correspond to geographical locations in maximum likelihood analyses. A sudden population expansion for South America is indicated by a mismatch distribution analysis, and further supported by significant (p<0.05) negative values of Fu and Li's D(F) and F, and Fu's F(S). This expansion, estimated at approximately 60 000 years BP (99 000-36 000 years BP 95% CI), encompasses a transition from a warm and dry time period prior to 50 000 years BP to an interval of maximum precipitation (50 000-36 000 years BP). Notably, this time period precedes the climatic and habitat changes associated with the last glacial maximum. In contrast, a multimodal distribution of haplotypes was observed for Central America suggesting either population equilibrium or a recent decline.
Significance: High levels of mitochondrial genetic diversity in combination with genetic differentiation among subgroups within regions and between regions highlight the importance of local population conservation in order to preserve maximal levels of genetic diversity in this species. Evidence of historically restricted female-mediated gene flow is an important consideration for captive-breeding programs.
RP Lerner, HRL (reprint author), Smithsonian Inst, Genet Lab, Natl Zool Pk, Washington, DC 20560 USA.
EM lernerh@si.edu
NR 95
TC 14
Z9 15
U1 2
U2 28
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD OCT 5
PY 2009
VL 4
IS 10
AR e7336
DI 10.1371/journal.pone.0007336
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 504DG
UT WOS:000270593600011
PM 19802391
ER
PT J
AU Graf, JA
Somers, MJ
Gunther, MS
Slotow, R
AF Graf, Jan A.
Somers, Michael J.
Gunther, Micaela Szykman
Slotow, Rob
TI Heterogeneity in the density of spotted hyaenas in Hluhluwe-iMfolozi
Park, South Africa
SO ACTA THERIOLOGICA
LA English
DT Article
DE call-ins; carnivore; Crocuta crocuta; playbacks; survey
ID HYENA CROCUTA-CROCUTA; WILD DOGS; NATIONAL-PARK; INTRAGUILD PREDATION;
POPULATION-DYNAMICS; ACINONYX-JUBATUS; NORTHERN RANGE; GROUP-SIZE; SPACE
USE; PREY
AB Animal population sizes and trends, as well as their distributions, are essential information to the understanding and conservation of ecosystems. During this study in Hluhluwe-iMfolozi Park, South Africa, a spotted hyaena Crocuta crocuta Erxleben, 1777 (Hyaenidae) population was surveyed by attracting individuals with pre-recorded sounds. The hyaena population (excluding cubs) is substantially larger (321 individuals) than the previous estimate of 200 and this population is the second largest protected population 2 in South Africa. Average hyaena density, at 0.357 individuals/km(2), was relatively high compared to other southern African conservation areas, and range from 0 to 1.25 individuals/km(2) across sampling stations. For short periods, spatial heterogeneity in density was marked at small and large spatial scales, but decreased when averaged over a longer period. This heterogeneity may be important in promoting the coexistence of other large and mobile carnivores in Hluhluwe-iMfolozi Park by creating potential dynamic competition refugia in space and time. Furthermore, heterogeneity of hyaena density at smaller scales should influence studies investigating the avoidance of hyaenas by competitively inferior carnivores.
C1 [Graf, Jan A.; Slotow, Rob] Univ KwaZulu Natal, Sch Biol & Conservat Sci, ZA-4041 Durban, South Africa.
[Somers, Michael J.] Univ Pretoria, Ctr Wildlife Management, Ctr Invas Biol, ZA-0002 Pretoria, South Africa.
[Gunther, Micaela Szykman] Smithsonian Inst, Ctr Species Survival, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA.
[Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA.
RP Graf, JA (reprint author), Univ KwaZulu Natal, Sch Biol & Conservat Sci, ZA-4041 Durban, South Africa.
EM janandreasgraf@yahoo.com
RI Somers, Michael/A-1523-2008;
OI Slotow, Rob/0000-0001-9469-1508; Szykman Gunther,
Micaela/0000-0002-7822-8094; /0000-0002-5836-8823
FU Green Trust (WWF-SA); Wildlands Conservation Trust; Endangered Wildlife
Trust; National Research Foundation; Smithsonian Institution; Sichel
Family Endowment; National Zoo; University of KwaZulu-Natal
FX We thank The Green Trust (WWF-SA), The Wildlands Conservation Trust, The
Endangered Wildlife Trust, National Research Foundation, Smithsonian
Institution, Sichel Family Endowment, Friends of the National Zoo, and
the University of KwaZulu-Natal for funding. We thank Ezemvelo KZN
Wildlife for permission to conduct this study. The managers and staff of
HiP and the Hluhluwe Research Centre are thanked for their extensive
logistical and material support. The numerous researchers and volunteers
at the Hluhluwe Research Centre and Mbuzane section outpost who
participated in the survey are thanked for their vital field assistance.
M. G. L. Mills is thanked for providing the hyaena audiotape. M. Lawes
is thanked for bootstrap statistical analysis. H. Olff, J. Cromsigt, and
R. and O. Howison, are thanked for assistance and advice on GIS
techniques. J. Cromsigt, M. Gusset and C. Gosling are thanked for
comments on an earlier draft of this manuscript.
NR 74
TC 6
Z9 7
U1 2
U2 7
PU POLISH ACAD SCIENCES
PI BIALOWIEZA
PA MAMMAL RESEARCH INST, 17-230 BIALOWIEZA, POLAND
SN 0001-7051
J9 ACTA THERIOL
JI Acta Theriol.
PD OCT
PY 2009
VL 54
IS 4
BP 333
EP 343
DI 10.4098/j.at.0001-7051.095.2008
PG 11
WC Zoology
SC Zoology
GA 505ZY
UT WOS:000270742800005
ER
PT J
AU Guatelli-Steinberg, D
Ferrell, RJ
Spence, J
Talabere, T
Hubbard, A
Schmidt, S
AF Guatelli-Steinberg, Debbie
Ferrell, Rebecca J.
Spence, Jennifer
Talabere, Tiffany
Hubbard, Amelia
Schmidt, Stacey
TI Sex Differences in Anthropoid Mandibular Canine Lateral Enamel Formation
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Article
DE sexual dimorphism; primate teeth; bimaturism
ID BODY-SIZE DIMORPHISM; LIFE-HISTORY; DENTAL DEVELOPMENT; FLUCTUATING
ASYMMETRY; CATARRHINE PRIMATES; EVOLUTION; ONTOGENY; HYPOPLASIA;
PATTERNS; STRESS
AB Previous research has demonstrated that great ape and macaque males achieve large canine crown sizes primarily through extended canine growth periods. Recent work has suggested, however, that platyrrhine males may achieve larger canine sizes by accelerating rather than prolonging growth. This study tested the hypothesis that the ontogenetic pathway leading to canine sexual dimorphism in catarrhines differs from that of platyrrhines. To test this hypothesis, males and females of several catarrhine genera (Hylobates, Papio, Macaca Cercopithecus, and Cercocebus) and three platyrrhine genera (Cebus, Ateles, and Callicebus) were compared in the number and spacing of perikymata (enamel growth increments) on their canine crowns. In addition, perikymata periodicities (the number of days of growth perikymata represent) were determined for five genera (Hylobates, Papio, Macaca, Cebus, and Ateles) using previously published as well as original data gathered for this study. The central findings are as follows: 1) males have more perikymata than females for seven of eight genera (in five of the seven, the differences are statistically significant); 2) in general, the greater the degree of sexual dimorphism, the greater the sex difference in male and female perikymata numbers; 3) there is no evidence of a systematic sex difference in primate periodicities; and 4) there is some evidence that sex differences in enamel formation rates may make a minor contribution to canine sexual dimorphism in Papio and Cercopithecus. These findings strongly suggest that in both catarrhines and platyrrhines prolongation of male canine growth is the primary mechanism by which canine crown sexual dimorphism is achieved. Am J Phys Anthropol 140:216-233, 2009. (C) 2009 Wiley-Liss, Inc.
C1 [Guatelli-Steinberg, Debbie; Spence, Jennifer; Talabere, Tiffany; Hubbard, Amelia; Schmidt, Stacey] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA.
[Ferrell, Rebecca J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
RP Guatelli-Steinberg, D (reprint author), Ohio State Univ, Dept Anthropol, 4034 Smith Lab,174 W 18th Ave, Columbus, OH 43210 USA.
EM guatelli-steinbe.1@osu.edu
FU National Science Foundation [BCS-0607520]
FX Grant sponsor: National Science Foundation; Grant number: BCS-0607520.
NR 40
TC 11
Z9 11
U1 1
U2 11
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0002-9483
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD OCT
PY 2009
VL 140
IS 2
BP 216
EP 233
DI 10.1002/ajpa.21047
PG 18
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 499CM
UT WOS:000270194200004
PM 19350641
ER
PT J
AU Mulhern, DM
Ubelaker, DH
AF Mulhern, Dawn M.
Ubelaker, Douglas H.
TI Bone Microstructure in Juvenile Chimpanzees
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Article
DE osteon; Hominoidea; histomorphometry; primate
ID REMODELING DYNAMICS; HAVERSIAN SYSTEMS; SECONDARY OSTEON;
PAN-TROGLODYTES; AGE; POPULATIONS; HISTOMORPHOMETRY; ALGORITHM;
PATTERNS; FEMUR
AB The growth, development, and maintenance of bone are influenced by genetic and environmental variables. Understanding variability in bone microstructure among primates may help illuminate the factors influencing the number and size of secondary osteons. The purpose of this study is to assess the bone microstructure in 8 humeral and 12 femoral sections of 12 juvenile chimpanzees, aged 2-15.3 years, and one adult chimp. Secondary osteons were counted and measured for 16 fields per section. Results indicate that the femur exhibits a mean osteon population density (OPD) of 4.46 +/- 2.34/mm(2), mean Haversian canal area of 0.0016 +/- 0.0007 mm(2), and mean osteon area of 0.033 +/- 0.006 mm(2). The humerus has a mean OPD of 4.72 +/- 1.57/mm(2), mean Haversian canal area of 0.0013 +/- 0.0003 mm(2), and mean osteon area of 0.033 +/- 0.005 mm(2). Differences are not significant between the humerus and femur, possibly indicating similar mechanical demands during locomotion. Osteon population density exhibits a moderate correlation with age (r = 0.498) in the femur of the juvenile chimps, but the adult chimp has an OPD of 10.28/mm(2), suggesting that osteons likely accumulate with age. Females exhibit higher osteon densities in the periosteal envelope compared to males in the humerus, indicating more remodeling during periosteal expansion. Overall similarities between chimpanzees and humans as well as previously published data on Late Pleistocene hominids (Abbott et al.: Am J Phys Anthropol 99 [1996] 585-601) suggest that bone microstructure has been stable throughout human evolution. Am J Phys Anthropol 140:368-375, 2009. (C) 2009 Wiley-Liss, Inc.
C1 [Mulhern, Dawn M.] Ft Lewis Coll, Dept Anthropol, Durango, CO 81301 USA.
[Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Mulhern, DM (reprint author), Ft Lewis Coll, Dept Anthropol, 1000 Rim Dr, Durango, CO 81301 USA.
EM mulhern_d@fortlewis.edu
NR 32
TC 7
Z9 7
U1 1
U2 5
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0002-9483
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD OCT
PY 2009
VL 140
IS 2
BP 368
EP 375
DI 10.1002/ajpa.20959
PG 8
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 499CM
UT WOS:000270194200017
PM 19434755
ER
PT J
AU Thitaram, C
Chansitthiwet, S
Pongsopawijit, P
Brown, JL
Wongkalasin, W
Daram, P
Roongsri, R
Kalmapijit, A
Mahasawangkul, S
Rojanasthien, S
Colenbrander, B
van der Weijden, GC
van Eerdenburg, FJCM
AF Thitaram, Chatchote
Chansitthiwet, Saran
Pongsopawijit, Pornsawan
Brown, Janine L.
Wongkalasin, Waroot
Daram, Prachayarat
Roongsri, Ronnachit
Kalmapijit, Anchalee
Mahasawangkul, Sittidet
Rojanasthien, Suvichai
Colenbrander, Ben
van der Weijden, Gysbert C.
van Eerdenburg, Frank J. C. M.
TI Use of genital inspection and female urine tests to detect oestrus in
captive Asian elephants
SO ANIMAL REPRODUCTION SCIENCE
LA English
DT Article
DE Oestrous cycle; Asian elephant; Genital inspection test; Urine test;
Pheromone
ID LOXODONTA-AFRICANA; CHEMICAL SIGNALS; REPRODUCTIVE-BEHAVIOR;
ESTROUS-CYCLE; DAIRY-COWS; MAXIMUS; COMMUNICATION; PHEROMONE; PREGNANCY;
FLEHMEN
AB Captive Asian elephant (Elephas maximus) populations are decreasing due to low birth rates compared to wild elephants. Improving oestrous detection in female elephants is required to ensure successful mating in captive and semi-captive herds. Responsive behaviours of eight semi-captive bull elephants to the uro-genital area (genital inspection test) or urinary pheromones (urine test) of 14 female elephants throughout the oestrous cycle were evaluated. Weekly blood samples were collected for 27 consecutive months (14 months for the genital inspection test and 13 months for the urine test) from female elephants to characterize the patterns of circulating progestagen. Responsive behaviours of bulls were compared between females in the follicular versus the luteal phase of the cycle. The sensitivity and specificity of the genital inspection test were 65% and 68%, while those of the urine test were 52% and 61%, respectively. The bulls showed significantly higher "genital inspection", "flehmen from genital area" and "trunk on back" behaviours during the genital inspection test, and "flehmen" behaviours during the urine test in oestrous than in non-oestrous females. In sum, this study showed that monitoring sexual behaviours of Asian elephant bulls towards females or their urine can be used to detect the oestrous period. Although the sensitivity and specificity of both tests were not as high as expected, still, these methods appear to be more efficient at detecting oestrous than traditional methods based on mahout estimations of female receptivity. The use of genital inspection and urine tests may lead to more successful matings and thus to creating self-sustaining populations of captive elephants in range countries. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Thitaram, Chatchote; Pongsopawijit, Pornsawan; Wongkalasin, Waroot; Daram, Prachayarat; Rojanasthien, Suvichai] Chiang Mai Univ, Fac Vet Med, Chiang Mai 50100, Thailand.
[Thitaram, Chatchote; Colenbrander, Ben; van der Weijden, Gysbert C.; van Eerdenburg, Frank J. C. M.] Univ Utrecht, Fac Vet Med, NL-3584 CL Utrecht, Netherlands.
[Chansitthiwet, Saran; Mahasawangkul, Sittidet] Forest Ind Org, Natl Elephant Inst, Thai Elephant Conservat Ctr, Lampang 52000, Thailand.
[Brown, Janine L.] Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA.
[Roongsri, Ronnachit; Kalmapijit, Anchalee] Maesa Elephant Camp, Chiang Mai 50100, Thailand.
RP Thitaram, C (reprint author), Chiang Mai Univ, Fac Vet Med, Chiang Mai 50100, Thailand.
EM thitaram@chiangmai.ac.th
FU National Research Council of Thailand; Royal Thai Government
scholarship, Thailand; Smithsonian Women's Committee, USA
FX We thank National Research Council of Thailand, Royal Thai Government
scholarship, Thailand, and the Smithsonian Women's Committee, USA for
research funding, Mr. Pichai Jirawattanapong, Utrecht University for
statistical assistance, Ms. Sue Walker, Ms. Karen Steinman, Ms. Nicole
Abbodanza from Smithsonian Conservation and Research Center for
endocrine laboratory support, Dr. Gannigar Nimtrakul, Chiang Mai zoo and
Mr. Kongphop Thilaongam for additional endocrine laboratory assistance,
Dr. Preecha Puangkham, Mr. Worawit Rojanaphaitoon, National Elephant
Institute, Mr. Choochart Kulmapijit, Maesa Elephant camp for allowing
long-term study of the elephants, all the mahouts and staffs of Thai
Elephant Conservation Center and Maesa Elephant camps for their
assistance.
NR 44
TC 1
Z9 2
U1 2
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-4320
J9 ANIM REPROD SCI
JI Anim. Reprod. Sci.
PD OCT
PY 2009
VL 115
IS 1-4
BP 267
EP 278
DI 10.1016/j.anireprosci.2008.11.017
PG 12
WC Agriculture, Dairy & Animal Science; Reproductive Biology
SC Agriculture; Reproductive Biology
GA 489KJ
UT WOS:000269418700027
PM 19131193
ER
PT J
AU Kettenring, KM
Whigham, DF
AF Kettenring, Karin M.
Whigham, Dennis F.
TI Seed viability and seed dormancy of non-native Phragmites australis in
suburbanized and forested watersheds of the Chesapeake Bay, USA
SO AQUATIC BOTANY
LA English
DT Article
DE Brackish wetland; Chesapeake Bay; Invasive species; Phragmites
australis; Seed dormancy; Seed germination; Seed viability
ID COMMON REED; SPARTINA-ALTERNIFLORA; COASTAL MARSH; SALT MARSHES;
GERMINATION; ESTABLISHMENT; DISPERSAL; INVASION; PLANTS; REPRODUCTION
AB The non-native, invasive haplotype of Phragmites australis is rapidly invading tidal and non-tidal wetlands across North America. Phragmites has the potential to spread by seeds and rhizomes. Seed viability and dormancy differences were quantified among 18 patches of non-native Phragmites in subestuarine wetlands in developed (i.e., suburbanized) vs. forested watersheds of the Chesapeake Bay. We used tetrazolium and germination assays to assess seed viability and compared germination percentages and rate of germination among fresh seeds, cold-moist treated seeds, and warm-dry treated seeds to evaluate seed dormancy. Seed viability was <1% in most patches but a few patches produced abundant viable seeds (5-21%). Seed viability, however, did not differ significantly between wetlands in forested vs. developed watersheds. Contrary to studies of Phragmites seed dormancy in European populations, some Phragmites seeds were dormant at maturity; cold-moist treated seeds germinated faster and to higher percentages than fresh seeds or warm-dry treated seeds. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Kettenring, Karin M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Kettenring, KM (reprint author), Utah State Univ, Ctr Ecol, 5210 Old Main Hill, Logan, UT 84322 USA.
EM karin.kettenring@usu.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU EPA STAR [692105]
FX We thank Jay O'Neill for assistance in the field and lab, Kelly Maloney
and Susan Durham for statistical advice, and Heather Baron for
developing the map in Fig. 1. We thank Elizabeth Stoffel of the American
Chestnut Land Trust for access to Parkers Creek. This research was
funded through a subcontract with Pennsylvania State University on EPA
STAR grant # 692105 to Denice Wardrop, Principal Investigator, and a
Smithsonian Postdoctoral Fellowship to KMK.
NR 41
TC 23
Z9 24
U1 9
U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3770
J9 AQUAT BOT
JI Aquat. Bot.
PD OCT
PY 2009
VL 91
IS 3
BP 199
EP 204
DI 10.1016/j.aquabot.2009.06.002
PG 6
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 498EL
UT WOS:000270119700012
ER
PT J
AU Bonanos, AZ
Massa, DL
Sewilo, M
Lennon, DJ
Panagia, N
Smith, LJ
Meixner, M
Babler, BL
Bracker, S
Meade, MR
Gordon, KD
Hora, JL
Indebetouw, R
Whitney, BA
AF Bonanos, A. Z.
Massa, D. L.
Sewilo, M.
Lennon, D. J.
Panagia, N.
Smith, L. J.
Meixner, M.
Babler, B. L.
Bracker, S.
Meade, M. R.
Gordon, K. D.
Hora, J. L.
Indebetouw, R.
Whitney, B. A.
TI SPITZER SAGE INFRARED PHOTOMETRY OF MASSIVE STARS IN THE LARGE
MAGELLANIC CLOUD
SO ASTRONOMICAL JOURNAL
LA English
DT Review
DE catalogs; galaxies: individual (LMC); infrared: stars; stars:
early-type; stars: emission-line, Be; stars: Wolf-Rayet
ID WOLF-RAYET STARS; O-TYPE STARS; GRAVITATIONAL LENSING EXPERIMENT;
BLANKETED MODEL ATMOSPHERES; EFFECTIVE TEMPERATURE SCALE; GIANT BRANCH
POPULATIONS; ECLIPSING BINARY-SYSTEM; LUMINOUS BLUE VARIABLES; YOUNG
STELLAR OBJECTS; LOCAL GROUP DWARFS
AB We present a catalog of 1750 massive stars in the Large Magellanic Cloud (LMC), with accurate spectral types compiled from the literature, and a photometric catalog for a subset of 1268 of these stars, with the goal of exploring their infrared properties. The photometric catalog consists of stars with infrared counterparts in the Spitzer SAGE survey database, for which we present uniform photometry from 0.3 to 24 mu m in the UBVIJHK(s)+IRAC+MIPS24 bands. The resulting infrared color-magnitude diagrams illustrate that the supergiant B[ e], red supergiant, and luminous blue variable (LBV) stars are among the brightest infrared point sources in the LMC, due to their intrinsic brightness, and at longer wavelengths, due to dust. We detect infrared excesses due to free-free emission among similar to 900 OB stars, which correlate with luminosity class. We confirm the presence of dust around 10 supergiant B[ e] stars, finding the shape of their spectral energy distributions (SEDs) to be very similar, in contrast to the variety of SED shapes among the spectrally variable LBVs. The similar luminosities of B[e] supergiants (log L/L-circle dot >= 4) and the rare, dusty progenitors of the new class of optical transients ( e. g., SN 2008S and NGC 300 OT), plus the fact that dust is present in both types of objects, suggests a common origin for them. We find the infrared colors for Wolf-Rayet stars to be independent of spectral type and their SEDs to be flatter than what models predict. The results of this study provide the first comprehensive roadmap for interpreting luminous, massive, resolved stellar populations in nearby galaxies at infrared wavelengths.
C1 [Bonanos, A. Z.; Massa, D. L.; Sewilo, M.; Lennon, D. J.; Panagia, N.; Smith, L. J.; Meixner, M.; Gordon, K. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, N.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Babler, B. L.; Bracker, S.; Meade, M. R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA.
RP Bonanos, AZ (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM bonanos@stsci.edu; massa@stsci.edu; sewilo@stsci.edu; lennon@stsci.edu;
panagia@stsci.edu; lsmith@stsci.edu; meixner@stsci.edu;
brian@sal.wisc.edu; s_bracker@hotmail.com; meade@sal.wisc.edu;
kgordon@stsci.edu; jhora@cfa.harvard.edu; remy@virginia.edu;
bwhitney@spacescience.org
RI Bonanos, Alceste/K-5392-2013;
OI Bonanos, Alceste/0000-0003-2851-1905; Lennon,
Daniel/0000-0003-3063-4867; Babler, Brian/0000-0002-6984-5752; Hora,
Joseph/0000-0002-5599-4650
NR 170
TC 75
Z9 74
U1 1
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 OCT
PY 2009
VL 138
IS 4
BP 1003
EP 1021
DI 10.1088/0004-6256/138/4/1003
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493WD
UT WOS:000269768500001
ER
PT J
AU Aigrain, S
Pont, F
Fressin, F
Alapini, A
Alonso, R
Auvergne, M
Barbieri, M
Barge, P
Borde, P
Bouchy, F
Deeg, H
De la Reza, R
Deleuil, M
Dvorak, R
Erikson, A
Fridlund, M
Gondoin, P
Guterman, P
Jorda, L
Lammer, H
Leger, A
Llebaria, A
Magain, P
Mazeh, T
Moutou, C
Ollivier, M
Patzold, M
Queloz, D
Rauer, H
Rouan, D
Schneider, J
Wuchter, G
Zucker, S
AF Aigrain, S.
Pont, F.
Fressin, F.
Alapini, A.
Alonso, R.
Auvergne, M.
Barbieri, M.
Barge, P.
Borde, P.
Bouchy, F.
Deeg, H.
De la Reza, R.
Deleuil, M.
Dvorak, R.
Erikson, A.
Fridlund, M.
Gondoin, P.
Guterman, P.
Jorda, L.
Lammer, H.
Leger, A.
Llebaria, A.
Magain, P.
Mazeh, T.
Moutou, C.
Ollivier, M.
Paetzold, M.
Queloz, D.
Rauer, H.
Rouan, D.
Schneider, J.
Wuchter, G.
Zucker, S.
TI Noise properties of the CoRoT data A planet-finding perspective
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: data analysis; techniques: photometric; stars: planetary
systems
ID STELLAR MICROVARIABILITY
AB In this short paper, we study the photometric precision of stellar light curves obtained by the CoRoT satellite in its planet-finding channel, with a particular emphasis on the time scales characteristic of planetary transits. Together with other articles in the same issue of this journal, it forms an attempt to provide the building blocks for a statistical interpretation of the CoRoT planet and eclipsing binary catch to date. After pre-processing the light curves so as to minimise long-term variations and outliers, we measure the scatter of the light curves in the first three CoRoT runs lasting more than 1 month, using an iterative non-linear filter to isolate signal on the time scales of interest. The behaviour of the noise on 2 h time scales is described well by a power-law with index 0.25 in R-magnitude, ranging from 0.1 mmag at R = 11.5 to 1 mmag at R = 16, which is close to the pre-launch specification, though still a factor 2-3 above the photon noise due to residual jitter noise and hot pixel events. There is evidence of slight degradation in the performance over time. We find clear evidence of enhanced variability on hour time scales (at the level of 0.5 mmag) in stars identified as likely giants from their R magnitude and B - V colour, which represent approximately 60 and 20% of the observed population in the directions of Aquila and Monoceros, respectively. On the other hand, median correlated noise levels over 2 h for dwarf stars are extremely low, reaching 0.05 mmag at the bright end.
C1 [Aigrain, S.; Pont, F.; Alapini, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Fressin, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Alonso, R.; Barbieri, M.; Barge, P.; Deleuil, M.; Guterman, P.; Jorda, L.; Llebaria, A.; Moutou, C.] Univ Aix Marseille 1, LAM, F-13388 Marseille, France.
[Auvergne, M.; Rouan, D.] Observ Paris, LESIA, F-92195 Meudon, France.
[Borde, P.; Leger, A.; Ollivier, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bouchy, F.] Observ Haute Provence, F-04870 St Michel lObservatoire, France.
[Deeg, H.] IAC, San Cristobal la Laguna 38205, Spain.
[De la Reza, R.] ON MCT, BR-20921030 Rio De Janeiro, Brazil.
[Dvorak, R.] Univ Vienna, IfA, A-1180 Vienna, Austria.
[Erikson, A.; Rauer, H.] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Fridlund, M.; Gondoin, P.] Estec, ESA, RSSD, NL-2200 Noordwijk, Netherlands.
[Lammer, H.] Austrian Acad Sci, IWF, A-8042 Graz, Austria.
[Magain, P.] Univ Liege, IAG, Liege 1, Belgium.
[Mazeh, T.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Paetzold, M.] Univ Cologne, RIU, D-50931 Cologne, Germany.
[Queloz, D.] Observ Geneva, CH-1290 Sauverny, Switzerland.
[Rauer, H.] Tech Univ Berlin, ZAA, D-10623 Berlin, Germany.
[Schneider, J.] Observ Paris, LUTH, F-92195 Meudon, France.
[Wuchter, G.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Zucker, S.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
RP Aigrain, S (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
EM suz@astro.ex.ac.uk
RI Alonso, Roi/D-8799-2014;
OI Alonso, Roi/0000-0001-8462-8126; Barbieri, Mauro/0000-0001-8362-3462
FU Spanish Science and Innovation ministry [ESP2007-65480-C02-02]; German
CoRoT team; DLR [50OW0204, 50OW0603, 50QP0701]; Israel Science
Foundation - Adler Foundation for Space Research [119/07]
FX H. D. acknowledges support from grant ESP2007-65480-C02-02 of the
Spanish Science and Innovation ministry, the German CoRoT team (TLS and
Univ. Cologne) from DLR grants 50OW0204, 50OW0603, and 50QP0701, and SZ
from the Israel Science Foundation - Adler Foundation for Space Research
(grant No. 119/07).
NR 12
TC 34
Z9 34
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 506
IS 1
BP 425
EP 429
DI 10.1051/0004-6361/200911885
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 509XN
UT WOS:000271052700045
ER
PT J
AU Giacintucci, S
Venturi, T
Brunetti, G
Dallacasa, D
Mazzotta, P
Cassano, R
Bardelli, S
Zucca, E
AF Giacintucci, S.
Venturi, T.
Brunetti, G.
Dallacasa, D.
Mazzotta, P.
Cassano, R.
Bardelli, S.
Zucca, E.
TI Testing the radio halo-cluster merger scenario The case of RXC
J2003.5-2323
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: clusters: general;
galaxies: clusters: individual: RXC J2003.5-2323
ID GALAXY CLUSTERS; DARK-MATTER; EMISSION; ORIGIN; REACCELERATION;
ACCELERATION; CONSTRAINTS; SAMPLE; RAYS; COMA
AB Aims. We present a combined radio, X-ray, and optical study of the galaxy cluster RXCJ2003.5-2323. The cluster hosts one of the largest, most powerful, and distant giant radio halos known to date, suggesting that it may be undergoing a strong merger. The aim of our multiwavelength study is to investigate the radio-halo cluster merger scenario.
Methods. We studied the radio properties of the giant radio halo in RXCJ2003.5-2323 by means of new radio data obtained at 1.4 GHz with the Very Large Array, and at 240 MHz with the Giant Metrewave Radio Telescope, in combination with previously published GMRT data at 610 MHz. The dynamical state of the cluster was investigated by means of X-ray Chandra observations and optical ESO-NTT observations.
Results. Our study confirms that RXCJ2003.5-2323 is an unrelaxed cluster. The unusual filamentary and clumpy morphology of the radio halo could be due to a combination of the filamentary structure of the magnetic field and turbulence in the inital stage of a cluster merger.
C1 [Giacintucci, S.; Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Giacintucci, S.; Venturi, T.; Brunetti, G.; Dallacasa, D.; Cassano, R.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Dallacasa, D.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Mazzotta, P.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Bardelli, S.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
RP Giacintucci, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM tventuri@ira.inaf.it
RI Zucca, Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015; Mazzotta,
Pasquale/B-1225-2016;
OI Zucca, Elena/0000-0002-5845-8132; Bardelli, Sandro/0000-0002-8900-0298;
Mazzotta, Pasquale/0000-0002-5411-1748; Cassano,
Rossella/0000-0003-4046-0637; Brunetti, Gianfranco/0000-0003-4195-8613;
Venturi, Tiziana/0000-0002-8476-6307
FU Italian Ministry of Foreign Affairs; MIUR [PRIN2004, PRIN2005, 2006,
PRIN-INAF2005]; [ASI-INAF I/023/05/01]
FX We thank the staff of the GMRT for their help during the observations.
The GMRT is run by the National Centre for Radio Astrophysics of the
Tata Institute of Fundamental Research. The optical data were obtained
with the European Southern Observatory NTT telescope, La Silla, Chile,
program 079. A-0191(A). We acknowledge financial contribution from the
Italian Ministry of Foreign Affairs, from MIUR grants PRIN2004, PRIN2005
and 2006, from PRIN-INAF2005 and from contract ASI-INAF I/023/05/01.
NR 27
TC 16
Z9 16
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 1
BP 45
EP 53
DI 10.1051/0004-6361/200912301
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502DU
UT WOS:000270436000006
ER
PT J
AU Giacintucci, S
Venturi, T
AF Giacintucci, S.
Venturi, T.
TI Tailed radio galaxies as tracers of galaxy clusters. Serendipitous
discoveries with the GMRT
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: clusters: general
ID MULTIFREQUENCY VLA OBSERVATIONS; ABELL CLUSTERS; HALO SURVEY; SKY
SURVEY; ANGLE; CATALOG; SAMPLE; BENT; SUBSTRUCTURE; REDSHIFTS
AB Aims. We report on the discovery of four new radio galaxies with tailed morphology. Tailed radio galaxies are generally found in rich environments, therefore their presence can be used as tracer of a cluster.
Methods. The radio galaxies were found in the fields of Giant Metrewave Radio Telescope (GMRT) observations carried out at 610 MHz and 327 MHz devoted to other studies. We inspected the literature and archives in the optical and X-ray bands to search for galaxy clusters or groups hosting them.
Results. All the tailed radio galaxies serendipitously found in the GMRT fields are located in rich environments. Two of them belong to the candidate cluster NCS J090232+204358, located at z(phot) = 0.0746; one belongs to the cluster MaxBCGJ 223.97317+22.15620 at z(phot) = 0.2619; finally we suggest that the fourth one is probing a galaxy cluster at z = 0.1177, located behind A262, and so far undetected in any band. Our results strengthen the relevance of high sensitivity and high resolution radio data in the detection of galaxy clusters at intermediate redshift.
C1 [Giacintucci, S.; Venturi, T.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Giacintucci, S (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
EM tventuri@ira.inaf.it
OI Venturi, Tiziana/0000-0002-8476-6307
FU Italian Ministry of Foreign Affairs; MIUR [PRIN2004, PRIN2005, 2006,
PRIN-INAF2005]; [ASI-INAF I/023/05/01]
FX We thank Prof. D. Dallacasa for insightful discussion and careful
reading of the manuscript and Dr. F. Gastaldello for discussion and help
in handling the X-ray data archives. We thank the staff of the GMRT for
their help during the observations. GMRT is run by the National Centre
for Radio Astrophysics of the Tata Institute of Fundamental Research. We
acknowledge financial contribution from the Italian Ministry of Foreign
Affairs, from MIUR grants PRIN2004, PRIN2005 and 2006, from
PRIN-INAF2005 and from contract ASI-INAF I/023/05/01.
NR 43
TC 5
Z9 5
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 1
BP 55
EP 61
DI 10.1051/0004-6361/200912609
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 502DU
UT WOS:000270436000007
ER
PT J
AU Guainazzi, M
Risaliti, G
Nucita, A
Wang, J
Bianchi, S
Soria, R
Zezas, A
AF Guainazzi, M.
Risaliti, G.
Nucita, A.
Wang, J.
Bianchi, S.
Soria, R.
Zezas, A.
TI AGN/starburst connection in action: the half million second RGS spectrum
of NGC 1365
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: starburst; X-rays:
galaxies; X-rays: individuals: NGC 1365
ID NARROW-LINE REGION; SOFT-X-RAY; REFLECTION GRATING SPECTROMETER;
SEYFERT-2 GALAXY NGC-1068; HUBBLE-SPACE-TELESCOPE; XMM-NEWTON LONG;
GALACTIC NUCLEI; PHYSICAL CONDITIONS; IONIZING-RADIATION; STARBURST
GALAXIES
AB Context. High-resolution X-ray observations in the imaging and spectral domain have recently opened a new window on active galactic nuclei (AGN) feedback onto the circumnuclear gas. Spectral diagnostics, as well as the remarkable morphological coincidence between [OIII] and X-rays, point to AGN photoionisation as the dominant ionisation mechanism on scales as large as a few kpc.
Aims. In this paper we extend these studies to the nearby Seyfert 2 galaxy NGC 1365, known to host a circumnuclear ring of intense star formation at similar or equal to 1.3 kpc from the nucleus. The main scope of this investigation is to study the connection between nuclear activity and star formation in nearby AGN.
Methods. We present a deep (similar or equal to 5.8 days) 0.3-2 keV high-resolution spectrum of NGC 1365, collected with the reflection grating spectrometer (RGS) on board XMM-Newton.
Results. The spectrum is dominated by strong recombination lines of He- and H-like transitions from carbon to silicon, as well as by L transitions from FeXVII. The continuum is strong, especially in the 10 to 20 angstrom range. Formal fits require two optically thin, collisionally ionised plasma components, with temperatures similar or equal to 300 and similar or equal to 640 eV. However, they leave the bulk of the forbidden components of the He-alpha OVII and NVI triplets unaccounted for. These features can be explained as being produced by photoionised gas. NGC 1365 is therefore the first obscured AGN, whose high-resolution X-ray spectrum requires both collisional ionisation and photoionisation.
Conclusions. The relative weakness of photoionisation does not stem from the intrinsic weakness of its AGN, whose X-ray luminosity is greater than or similar to 10(42) erg s(-1). We suggest that it may instead come from the line-of-sight from the active nucleus to the NLR being blocked by optically thick matter in the broad line region, at the same time responsible for the large observed variation of the column density obscuring the X-ray active nucleus. Alternatively, NGC 1365 could host a remarkably luminous nuclear starburst when compared to the AGN accretion power.
C1 [Guainazzi, M.; Nucita, A.] ESA, European Space Astron Ctr, Madrid 28691, Spain.
[Risaliti, G.; Wang, J.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA.
[Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Bianchi, S.] Univ Rome, Dipartimento Fis, I-00146 Rome, Italy.
[Soria, R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
RP Guainazzi, M (reprint author), ESA, European Space Astron Ctr, POB 78, Madrid 28691, Spain.
EM Matteo.Guainazzi@sciops.esa.int
RI Wang, Junfeng/A-1476-2011; Bianchi, Stefano/B-4804-2010; Zezas,
Andreas/C-7543-2011;
OI Bianchi, Stefano/0000-0002-4622-4240; Zezas,
Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X
FU National Aeronautics and Space Administration
FX Based on observations obtained with XMM-Newton, an ESA science mission
with instruments and contributions directly funded by ESA Member States
and NASA This research has made use of data obtained through the High
Energy Astrophysics Science Archive Research Centre Online Service,
provided by the NASA/Goddard Space Flight Centre and 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. A careful reading of the
original manuscript by an anonymous referee is gratefully acknowledged.
NR 74
TC 24
Z9 24
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 2
BP 589
EP 600
DI 10.1051/0004-6361/200912758
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 504ST
UT WOS:000270638600014
ER
PT J
AU Huber, D
Matthews, JM
Croll, B
Obbrugger, M
Gruberbauer, M
Guenther, DB
Weiss, WW
Rowe, JF
Kallinger, T
Kuschnig, R
Scholtz, AL
Moffat, AFJ
Rucinski, SM
Sasselov, D
Walker, GAH
AF Huber, D.
Matthews, J. M.
Croll, B.
Obbrugger, M.
Gruberbauer, M.
Guenther, D. B.
Weiss, W. W.
Rowe, J. F.
Kallinger, T.
Kuschnig, R.
Scholtz, A. L.
Moffat, A. F. J.
Rucinski, S. M.
Sasselov, D.
Walker, G. A. H.
TI A search for p-modes and other variability in the binary system 85
Pegasi using MOST photometry
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: photometric; stars: individual: 85 Peg; stars: oscillations;
stars: rotation; starspots; binaries: general
ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; LINE-DATA-BASE;
DIFFERENTIAL ROTATION; STELLAR OSCILLATIONS; ABUNDANCE ANALYSIS;
EPSILON-OPHIUCHI; ASTEROSEISMOLOGY; GRANULATION; SPACE
AB Context. Asteroseismology has great potential for the study of metal-poor stars due to its sensitivity to determine stellar ages. Solid detections of oscillation frequencies in stars with well constrained fundamental parameters, combined with a known rotation period, should significantly advance our understanding of stellar structure and evolution in context with metallicity effects.
Aims. Our goal was to detect p-mode oscillations in the metal-poor sub-dwarf 85 Peg A and to search for variability on longer timescales.
Methods. We have obtained continuous high-precision optical photometry of the binary system 85 Pegasi with the MOST (Microvariability & Oscillations of STars) space telescope in two seasons (2005 & 2007). The light curves were analyzed using traditional Fourier techniques. Furthermore, we redetermined v sin i for 85 Peg A using high resolution spectra obtained through the ESO archive, and used photometric spot modeling to interpret long periodic variations.
Results. Our frequency analysis yields no convincing evidence for p-modes significantly above a noise level of 4 ppm. Using simulated p-mode patterns we provide upper rms amplitude limits for 85 Peg A. After removal of instrumental trends the light curve shows evidence for variability with a period of about 11 d and this periodicity is also seen in the follow up run in 2007; however, as different methods to remove instrumental trends in the 2005 run yield vastly different results, the exact shape and periodicity of the 2005 variability remain uncertain. Our re-determined v sin i value for 85 Peg A is comparable to previous studies and we provide realistic uncertainties for this parameter. Using these values in combination with simple photometric spot models we are able to reconstruct the observed variations.
Conclusions. The null-detection of p-modes in 85 Peg A is consistent with theoretical values for pulsation amplitudes in this star. The detected long-periodic variation in the 85 Peg system must await confirmation by further observations with similar or better precision and long-term stability. If the 11 d periodicity is real, rotational modulation of surface features on one of the components is the most likely explanation.
C1 [Huber, D.; Obbrugger, M.; Gruberbauer, M.; Weiss, W. W.; Kallinger, T.; Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Matthews, J. M.; Kallinger, T.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Croll, B.; Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Gruberbauer, M.; Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Rowe, J. F.] NASA, Moffett Field, CA 94035 USA.
[Scholtz, A. L.] Vienna Univ Technol, Inst Commun & Radiofrequency Engn, A-1040 Vienna, Austria.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Huber, D (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM huber@astro.univie.ac.at
FU Natural Sciences & Engineering Research Council (NSERC) Canada
FX We are grateful for discussions with Pierre Demarque. We are also
thankful to Gerald Handler for critical discussions concerning the
p-mode detection limit. M. G., M.O., T. K., W. W. W. and R. K. are
supported by the Austrian Fonds zur Forderung der wissenschaftlichen
Forschung, project number P17580-N02. The Austrian participation in the
MOST project is funded by the Austrian Research Promotion Agency (FFG).
B. C., D. B. G., J.M.M., A.F.J.M., and S. R. acknowledge funding from
the Natural Sciences & Engineering Research Council (NSERC) Canada.
NR 60
TC 1
Z9 1
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 2
BP 715
EP 725
DI 10.1051/0004-6361/200912139
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 504ST
UT WOS:000270638600027
ER
PT J
AU Marcaide, JM
Marti-Vidal, I
Alberdi, A
Perez-Torres, MA
Ros, E
Diamond, PJ
Guirado, JC
Lara, L
Shapiro, II
Stockdale, CJ
Weiler, KW
Mantovani, F
Preston, RA
Schilizzi, RT
Sramek, RA
Trigilio, C
Van Dyk, SD
Whitney, AR
AF Marcaide, J. M.
Marti-Vidal, I.
Alberdi, A.
Perez-Torres, M. A.
Ros, E.
Diamond, P. J.
Guirado, J. C.
Lara, L.
Shapiro, I. I.
Stockdale, C. J.
Weiler, K. W.
Mantovani, F.
Preston, R. A.
Schilizzi, R. T.
Sramek, R. A.
Trigilio, C.
Van Dyk, S. D.
Whitney, A. R.
TI A decade of SN 1993J: discovery of radio wavelength effects in the
expansion rate
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: individual: M 81; radio continuum: stars;
supernovae: general; supernovae: individual: SN 1993J; techniques:
interferometric
ID HUBBLE-SPACE-TELESCOPE; IIB SUPERNOVA 1993J; CIRCUMSTELLAR INTERACTION;
OPTICAL-SPECTRA; SN-1993J VLBI; NEBULAR PHASE; LIGHT CURVES; MASS-LOSS;
X-RAYS; M81
AB We studied the growth of the shell-like radio structure of supernova SN1993J in M 81 from September 1993 to October 2003 with very-long-baseline interferometry (VLBI) observations at the wavelengths of 3.6, 6, and 18 cm. We developed a method to accurately determine the outer radius (R) of any circularly symmetric compact radio structure such as SN1993J.
The source structure of SN 1993J remains circularly symmetric (with deviations from circularity under 2%) over almost 4000 days. We characterize the decelerated expansion of SN 1993J until approximately day 1500 after explosion with an expansion parameter m = 0.845 +/- 0.005 (R proportional to t(m)). However, from that day onwards the expansion differs when observed at 6 and 18 cm. Indeed, at 18 cm, the expansion can be well characterized by the same m as before day 1500, while at 6 cm the expansion appears more decelerated, and is characterized by another expansion parameter, m(6) = 0.788 +/- 0.015. Therefore, since about day 1500 onwards, the radio source size has been progressively smaller at 6 cm than at 18 cm. These findings differ significantly from those of other authors in the details of the expansion. In our interpretation, the supernova expands with a single expansion parameter, m = 0.845 +/- 0.005, and the 6 cm results beyond day 1500 are caused by physical effects, perhaps also coupled to instrumental limitations. Two physical effects may be involved: (a) a changing opacity of the ejecta to the 6 cm radiation; and (b) a radial decrease of the magnetic field in the emitting region.
We also found that at 6 cm about 80% of the radio emission from the backside of the shell behind the ejecta is absorbed (our average estimate, since we cannot determine any possible evolution of the opacity), and the width of the radio shell is (31 +/- 2)% of the outer radius. The shell width at 18 cm depends on the degree of assumed absorption. For 80% absorption, the width is (33.5 +/- 1.7)%, and for 100% absorption, it is (37.8 +/- 1.3)%.
A comparison of our VLBI results with optical spectral line velocities shows that the deceleration is more pronounced in the radio than in the optical. This difference might be due to a progressive penetration of ejecta instabilities into the shocked circumstellar medium, as also suggested by other authors.
C1 [Marcaide, J. M.; Marti-Vidal, I.; Perez-Torres, M. A.; Ros, E.; Guirado, J. C.] Univ Valencia, Dept Astron, Valencia, Spain.
[Marti-Vidal, I.; Ros, E.] Max Planck Inst Radioastron, D-5300 Bonn, Germany.
[Alberdi, A.; Perez-Torres, M. A.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Diamond, P. J.] Univ Manchester, Jodrell Bank Observ, Manchester, Lancs, England.
[Lara, L.] Univ Granada, Granada, Spain.
[Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stockdale, C. J.] Marquette Univ, Milwaukee, WI 53233 USA.
[Weiler, K. W.] USN, Res Lab, Washington, DC 20375 USA.
[Mantovani, F.] INAF, Ist Radioastron, Bologna, Italy.
[Preston, R. A.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Schilizzi, R. T.] Int SKA Project Off, Dwingeloo, Netherlands.
[Sramek, R. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Trigilio, C.] INAF, Ist Radioastron, Noto, Italy.
[Van Dyk, S. D.] Spitzer Sci Ctr, Pasadena, CA USA.
[Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA.
RP Marcaide, JM (reprint author), Univ Valencia, Dept Astron, Valencia, Spain.
EM J.M.Marcaide@uv.es
RI Marti-Vidal, Ivan/A-8799-2017;
OI Marti-Vidal, Ivan/0000-0003-3708-9611; Ros, Eduardo/0000-0001-9503-4892;
Van Dyk, Schuyler/0000-0001-9038-9950
NR 79
TC 22
Z9 22
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 3
BP 927
EP 945
DI 10.1051/0004-6361/200912133
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508DF
UT WOS:000270907100001
ER
PT J
AU Sauter, J
Wolf, S
Launhardt, R
Padgett, DL
Stapelfeldt, KR
Pinte, C
Duchene, G
Menard, F
McCabe, CE
Pontoppidan, K
Dunham, M
Bourke, TL
Chen, JH
AF Sauter, J.
Wolf, S.
Launhardt, R.
Padgett, D. L.
Stapelfeldt, K. R.
Pinte, C.
Duchene, G.
Menard, F.
McCabe, C. -E.
Pontoppidan, K.
Dunham, M.
Bourke, T. L.
Chen, J. -H.
TI The circumstellar disc in the Bok globule CB 26 Multi-wavelength
observations and modelling of the dust disc and envelope
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; planetary systems: protoplanetary disks; radiative
transfer; stars: formation; stars: individual: CB 26
ID MULTIBAND IMAGING PHOTOMETER; TAURI CIRCUMBINARY RING; MU-M;
RADIATIVE-TRANSFER; ABSOLUTE CALIBRATION; GG-TAURI; SIZE DISTRIBUTION;
BUTTERFLY STAR; SPITZER; EXTINCTION
AB Context. Circumstellar discs are expected to be the nursery of planets. Grain growth within such discs is the first step in the planet formation process. The Bok globule CB 26 harbours such a young disc.
Aims. We present a detailed model of the edge-on circumstellar disc and its envelope in the Bok globule CB 26.
Methods. The model is based on HST near-infrared maps in the I, J, H, and K bands, OVRO and SMA radio maps at 1.1 mm, 1.3 mm and 2.7 mm, and the spectral energy distribution (SED) from 0.9 mu m to 3 mm. New photometric and spectroscopic data from the Spitzer Space Telescope and the Caltech Submilimeter Observatory are also part of our analysis. Using the self-consistent radiative transfer code MC3D, the model we construct is able to discriminate between parameter sets and dust properties of both envelope and disc.
Results. We find that the data are fit by a disc that has an inner hole with a radius of 45 +/- 5 AU. Based on a dust model including silicate and graphite, the maximum grain size needed to reproduce the spectral millimetre index is 2.5 mu m. Features seen in the near-infrared images, dominated by scattered light, can be described as a result of a rotating envelope.
Conclusions. Successful employment of ISM dust in both the disc and envelope hint that grain growth may not yet play a significant role for the appearance of this system. A large inner hole implies that CB 26 is a circumbinary disc.
C1 [Sauter, J.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Sauter, J.; Launhardt, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Pontoppidan, K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Pinte, C.; Duchene, G.; Menard, F.] UJF, CNRS, Lab Astrophys Grenoble, CNRS,UMR 5571, F-38041 Grenoble 9, France.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dunham, M.; Chen, J. -H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Sauter, J (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24098 Kiel, Germany.
EM jsauter@mpia.de
RI Stapelfeldt, Karl/D-2721-2012
FU DFG [759]; CNRS/INSU, France; Agence Nationale pour la Recherche of
France [ANR-07-BLAN-0221]; NASA [10603, 30765]; European Commission
[PIEF-GA2008-220891]; Smithsonian Institution; Academia Sinica
FX The authors thank all members of the GEODE-team for their help in this
project. J. Sauter thanks Owen Matthews, Jens Rodmann, and Arjan Bik for
enlightening discussions. This work is supported by the DFG through the
research group 759 "The Formation of Planets: The Critical First Growth
Phase". F. Menard thanks financial support from Programme national de
Physique Stellaire (PNPS) of CNRS/INSU, France and from Agence Nationale
pour la Recherche of France under contract ANR-07-BLAN-0221. This work
has been supported by NASA funding from the Space Telescope Science
Institute, HST general observer program 10603; and by NASA funding from
the Jet Propulsion Laboratory, under Spitzer general observer program
30765. C. Pinte acknowledges the funding from the European Commission's
Seventh Framework Program as a Marie Curie Intra-European Fellow
(PIEF-GA2008-220891). The Submillimeter Array is a joint project between
the Smithsonian Astrophysical Observatory and the Academia Sinica
Institute of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica.
NR 61
TC 29
Z9 29
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2009
VL 505
IS 3
BP 1167
EP 1182
DI 10.1051/0004-6361/200912397
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 508DF
UT WOS:000270907100020
ER
PT J
AU Drake, JJ
Ratzlaff, PW
Laming, JM
Raymond, J
AF Drake, Jeremy J.
Ratzlaff, Peter W.
Laming, J. Martin
Raymond, John
TI AN ABSENCE OF X-RAY ACCRETION SHOCK INSTABILITY SIGNATURES IN TW HYDRAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: formation; stars: individual (TW hydrae);
X-rays: stars
ID YOUNG STELLAR OBJECTS; TAURI-STARS; MAGNETOSPHERIC ACCRETION;
MAGNETIC-FIELDS; EMISSION-LINES; PHOTOMETRIC VARIABILITY; ROTATION
PERIODS; RADIATIVE SHOCKS; ATOMIC DATABASE; DISK ACCRETION
AB Gas accreting onto T Tauri stars should form shocks that are susceptible to the classical radiative shock instability. The instability should give rise to strong periodic modulation in the X-ray emission from the shock-heated plasma. Time series analysis of soft X-rays thought to arise predominantly in an accretion shock on the classical T Tauri star TW Hydrae reveals no periodic variations and a 99% confidence pulsed fraction limit of 5% over the frequency range 0.0001-6.81 Hz. We find no clear explanation for the absence of X-ray instability signatures, but suggest that existing one-dimensional models are too simple to explain the three-dimensional shock structure, or that preheating and deceleration of the accretion stream by the damping of magnetohydrodynamic waves excited either by the shock itself, or more deeply in the stellar envelope, could ameliorate the instability in the likely case of a sub-Alfvenic shock.
C1 [Drake, Jeremy J.; Ratzlaff, Peter W.; Raymond, John] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Laming, J. Martin] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA.
EM jdrake@cfa.harvard.edu
FU NASA [NAS8-39073]; CXC
FX J.D. and P. R. were supported by NASA contract NAS8-39073 to the Chandra
X-ray Center during the course of this research and thank the director,
H. Tananbaum, and the CXC science staff for advice and support.
NR 70
TC 18
Z9 18
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 1224
EP 1229
DI 10.1088/0004-637X/703/2/1224
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500005
ER
PT J
AU Klaassen, PD
Wilson, CD
Keto, ER
Zhang, Q
AF Klaassen, P. D.
Wilson, C. D.
Keto, E. R.
Zhang, Q.
TI ROTATION OF THE WARM MOLECULAR GAS SURROUNDING ULTRACOMPACT HII REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: kinematics and dynamics; molecular data; stars: formation;
submillimeter
ID STAR-FORMING REGIONS; W51 MASSIVE CORES; METHYL CYANIDE; TRIGONOMETRIC
PARALLAXES; DYNAMICAL COLLAPSE; SULFUR CHEMISTRY; RADIO-CONTINUUM;
ACCRETION DISK; YOUNG STARS; HOT CORES
AB We present molecular line and 1.4 mm continuum observations toward five massive star-forming regions at arcsecond resolution using the Submillimeter Array. We find that the warm molecular gas surrounding each HII region (as traced by SO(2) and OCS) appears to be undergoing bulk rotation. From the molecular line emission and thermal component of the continuum emission, we independently derived gas masses for each region which are consistent with each other. From the free-free component of the continuum emission, we estimate the minimum stellar mass required to power the H II region and find that this mass, when added to the derived gas mass, is a significant fraction of the dynamical mass for that region.
C1 [Klaassen, P. D.; Wilson, C. D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Keto, E. R.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM pklaasse@eso.org
OI Zhang, Qizhou/0000-0003-2384-6589
FU National Science and Engineering Research Council of Canada (NSERC)
FX We acknowledge the support of the National Science and Engineering
Research Council of Canada (NSERC). We also thank our anonymous referee
whose insights greatly improved this manuscript.
NR 52
TC 33
Z9 33
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 1308
EP 1317
DI 10.1088/0004-637X/703/2/1308
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500012
ER
PT J
AU Sollerman, J
Mortsell, E
Davis, TM
Blomqvist, M
Bassett, B
Becker, AC
Cinabro, D
Filippenko, AV
Foley, RJ
Frieman, J
Garnavich, P
Lampeitl, H
Marriner, J
Miquel, R
Nichol, RC
Richmond, MW
Sako, M
Schneider, DP
Smith, M
Vanderplas, JT
Wheeler, JC
AF Sollerman, J.
Mortsell, E.
Davis, T. M.
Blomqvist, M.
Bassett, B.
Becker, A. C.
Cinabro, D.
Filippenko, A. V.
Foley, R. J.
Frieman, J.
Garnavich, P.
Lampeitl, H.
Marriner, J.
Miquel, R.
Nichol, R. C.
Richmond, M. W.
Sako, M.
Schneider, D. P.
Smith, M.
Vanderplas, J. T.
Wheeler, J. C.
TI FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II (SDSS-II) SUPERNOVA RESULTS:
CONSTRAINTS ON NONSTANDARD COSMOLOGICAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; supernovae: general
ID ANISOTROPY-PROBE OBSERVATIONS; DARK ENERGY CONSTRAINTS;
HUBBLE-SPACE-TELESCOPE; IA SUPERNOVAE; LAMBDA; DISCOVERIES
AB We use the new Type Ia supernovae discovered by the Sloan Digital Sky Survey-II supernova survey, together with additional supernova data sets as well as observations of the cosmic microwave background and baryon acoustic oscillations to constrain cosmological models. This complements the standard cosmology analysis presented by Kessler et al. in that we discuss and rank a number of the most popular nonstandard cosmology scenarios. When this combined data set is analyzed using the MLCS2k2 light-curve fitter, we find that more exotic models for cosmic acceleration provide a better fit to the data than the.CDM model. For example, the flat Dvali-Gabadadze-Porrati model is ranked higher by our information-criteria (IC) tests than the standard model with a flat universe and a cosmological constant. When the supernova data set is instead analyzed using the SALT-II light-curve fitter, the standard cosmological-constant model fares best. This investigation of how sensitive cosmological model selection is to assumptions about, and within, the light-curve fitters thereby highlights the need for an improved understanding of these unresolved systematic effects. Our investigation also includes inhomogeneous Lemaitre-Tolman-Bondi (LTB) models. While our LTB models can be made to fit the supernova data as well as any other model, the extra parameters they require are not supported by our IC analysis. Finally, we explore more model-independent ways to investigate the cosmic expansion based on this new data set.
C1 [Sollerman, J.; Davis, T. M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Copenhagen, Denmark.
[Sollerman, J.; Blomqvist, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Mortsell, E.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Blomqvist, M.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Bassett, B.; Smith, M.] S African Astron Observ, ZA-7935 Obervatory, South Africa.
[Bassett, B.; Smith, M.] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa.
[Becker, A. C.; Vanderplas, J. T.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Cinabro, D.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48202 USA.
[Filippenko, A. V.; Foley, R. J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Frieman, J.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Frieman, J.; Marriner, J.] Fermilab Natl Accelerator Lab, Ctr Astrophys, Batavia, IL 60510 USA.
[Garnavich, P.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Lampeitl, H.; Nichol, R. C.; Smith, M.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Miquel, R.] Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Richmond, M. W.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
[Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Sollerman, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, Copenhagen, Denmark.
RI Davis, Tamara/A-4280-2008;
OI Miquel, Ramon/0000-0002-6610-4836; Davis, Tamara/0000-0002-4213-8783;
Sollerman, Jesper/0000-0003-1546-6615
NR 44
TC 95
Z9 95
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 1374
EP 1385
DI 10.1088/0004-637X/703/2/1374
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500019
ER
PT J
AU Bogdanov, S
Grindlay, JE
AF Bogdanov, Slavko
Grindlay, Jonathan E.
TI DEEP XMM-NEWTON SPECTROSCOPIC AND TIMING OBSERVATIONS OF THE ISOLATED
RADIO MILLISECOND PULSAR PSR J0030+0451
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; pulsars: individual (PSR J0030+0451); relativity;
stars: neutron; X-rays: stars
ID ROTATING NEUTRON-STARS; X-RAY OBSERVATIONS; LIGHT CURVES; EMISSION;
PSR-J0030+0451; ATMOSPHERES; J0437-4715; TELESCOPE; RADIATION; NEBULA
AB We present deep XMM-Newton European Photon Imaging Camera spectroscopic and timing X-ray observations of the nearby solitary radio millisecond pulsar, PSR J0030+0451. Its emission spectrum in the 0.1-10 keV range is found to be remarkably similar to that of the nearest and best-studied millisecond pulsar, PSR J0437-4715, being well described by a predominantly thermal two-temperature model plus a faint hard tail evident above similar to 2 keV. The pulsed emission in the 0.3-2 keV band is characterized by two broad pulses with pulsed fraction similar to 60%-70%, consistent with a mostly thermal origin of the X-rays only if the surface polar cap radiation is from a light-element atmosphere. Modeling of the thermal pulses permits us to place constraints on the neutron star radius of R > 10.7 (95% confidence) and R > 10.4 km (at 99.9% confidence) for M = 1.4 M(circle dot).
C1 [Bogdanov, Slavko; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bogdanov, Slavko] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
RP Bogdanov, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sbogdanov@cfa.harvard.edu; josh@cfa.harvard.edu
OI Bogdanov, Slavko/0000-0002-9870-2742
FU XMM-Newton Guest Observer NASA [NNX08AD54G]; Canadian Institute for
Advanced Research Junior Fellowship; ESA Member States; NASA; NASA
Astrophysics Data System (ADS)
FX We thank A. Lommen for providing the radio pulse profile of PSR
J0030+0451 and the anonymous referee for offering numerous helpful
comments. The research presented was funded in part by XMM-Newton Guest
Observer NASA grant NNX08AD54G awarded through the Harvard College
Observatory. S. B. is supported in part by a Lorne Trottier Research
Chair Fellowship and a Canadian Institute for Advanced Research Junior
Fellowship. This work was based on observations obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. The research in this
paper has made use of the NASA Astrophysics Data System (ADS).
NR 31
TC 26
Z9 26
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 1557
EP 1564
DI 10.1088/0004-637X/703/2/1557
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500030
ER
PT J
AU Savcheva, A
van Ballegooijen, A
AF Savcheva, Antonia
van Ballegooijen, Adriaan
TI NONLINEAR FORCE-FREE MODELING OF A LONG-LASTING CORONAL SIGMOID
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: magnetic fields; Sun: X-rays, gamma rays
ID SOHO EIT OBSERVATIONS; SOLAR ACTIVE REGIONS; MAGNETIC-FLUX ROPES; X-RAY
TELESCOPE; KINK INSTABILITY; MASS EJECTIONS; FILAMENT CHANNELS; YOHKOH
SXT; FIELDS; FLARES
AB A study of the magnetic configuration and evolution of a long-lasting quiescent coronal sigmoid is presented. The sigmoid was observed by Hinode/XRT and Transition Region and Coronal Explorer (TRACE) between 2007 February 6 and 12 when it finally erupted. We construct nonlinear force-free field models for several observations during this period, using the flux-rope insertion method. The high spatial and temporal resolution of the X-Ray Telescope (XRT) allows us to finely select best-fit models that match the observations. The modeling shows that a highly sheared field, consisting of a weakly twisted flux rope embedded in a potential field, very well describes the structure of the X-ray sigmoid. The flux rope reaches a stable equilibrium, but its axial flux is close to the stability limit of about 5 x 10(20) Mx. The relative magnetic helicity increases with time from February 8 until just prior to the eruption on February 12. We study the spatial distribution of the torsion parameter a in the vicinity of the flux rope, and find that it has a hollow-core distribution, i.e., electric currents are concentrated in a current layer at the boundary between the flux rope and its surroundings. The current layer is located near the bald patch separatrix surface (BPSS) of the magnetic configuration, and the X-ray emission appears to come from this current layer/BPSS, consistent with the Titov and Demoulin model. We find that the twist angle F of the magnetic field increases with time to about 2 pi just prior to the eruption, but never reaches the value necessary for the kink instability.
C1 [Savcheva, Antonia; van Ballegooijen, Adriaan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Savcheva, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM asavcheva@cfa.harvard.edu
OI van Ballegooijen, Adriaan/0000-0002-5622-3540
FU ESA; NSC (Norway); NASA [NNM07AB07C]
FX Hinode is a Japanese mission developed, launched, and operated by
ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). Additional
operational support is provided by ESA, NSC (Norway). This work was
supported by NASA contract NNM07AB07C to SAO. We also thank the referee
for very useful comments which helped making this work better.
NR 63
TC 45
Z9 45
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 1766
EP 1777
DI 10.1088/0004-637X/703/2/1766
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500046
ER
PT J
AU Gelfand, JD
Slane, PO
Zhang, WQ
AF Gelfand, Joseph D.
Slane, Patrick O.
Zhang, Weiqun
TI A DYNAMICAL MODEL FOR THE EVOLUTION OF A PULSAR WIND NEBULA INSIDE A
NONRADIATIVE SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; supernova remnants
ID RELATIVISTIC MHD SIMULATIONS; RAYLEIGH-TAYLOR INSTABILITY;
X-RAY-EMISSION; CRAB-NEBULA; NEUTRON-STARS; MAGNETIC-FIELD; COSMIC-RAYS;
VELA; ORIGIN; ACCELERATION
AB A pulsar wind nebula (PWN) inside a supernova remnant provides a unique insight into the properties of the central neutron star, the relativistic wind powered by its loss of rotational energy, its progenitor supernova, and the surrounding environment. In this paper, we present a new semianalytic model for the evolution of such a PWN throughout its lifetime. This model couples the dynamical and radiative evolution of the PWNe, and predicts both the dynamical (e. g., radius and expansion velocity) and radiative (radio to TeV gamma-ray spectrum) properties of the PWN during this period. As a result, it is well suited for using the observed properties of a PWN to constrain the physical characteristics of the neutron star, pulsar wind, progenitor supernova, and surrounding environment. We also discuss the expected evolution for a particular set of these parameters, and show that it reproduces the large spectral break inferred from the radio and X-ray spectrum of many young PWNe, and the low break frequency, low radio luminosity, high TeV gamma-ray luminosity, and high magnetization observed for several older PWNe. The predicted spectrum of this PWN also contains spectral features which appear during different evolutionary phases detectable with new radio and gamma-ray observing facilities such as the Extended Very Large Array and the Fermi Gamma-ray Space Telescope. Finally, this model has implications for determining if PWNe can inject a sufficient number of energetic electrons and positrons into their surroundings to explain the recent measurements of the cosmic-ray positron fraction by PAMELA and the cosmic-ray lepton spectrum by ATIC and HESS.
C1 [Gelfand, Joseph D.; Zhang, Weiqun] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gelfand, JD (reprint author), New York Univ, Ctr Cosmol & Particle Phys, Meyer Hall Phys,4 Washington Pl, New York, NY 10003 USA.
RI Gelfand, Joseph/F-1110-2015
OI Gelfand, Joseph/0000-0003-4679-1058
FU NSF [AST-0702957]
FX We thank Roger Chevalier, Andrei Gruzinov, Andrew MacFadyen, and Matias
Zaldariagga for useful discussions, and the anonymous referee for useful
comments. J. D. G. is supported by an NSF Astronomy and Astrophysics
Postdoctoral Fellowship under award AST-0702957.
NR 66
TC 63
Z9 63
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2009
VL 703
IS 2
BP 2051
EP 2067
DI 10.1088/0004-637X/703/2/2051
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495XS
UT WOS:000269929500072
ER
PT J
AU Jimenez-Serra, I
Martin-Pintado, J
Caselli, P
Martin, S
Rodriguez-Franco, A
Chandler, C
Winters, JM
AF Jimenez-Serra, I.
Martin-Pintado, J.
Caselli, P.
Martin, S.
Rodriguez-Franco, A.
Chandler, C.
Winters, J. M.
TI UNVEILING THE MAIN HEATING SOURCES IN THE CEPHEUS A HW2 REGION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual (Cepheus A); ISM: molecules; stars: formation
ID THERMAL RADIO JET; A HW2; HIGH-RESOLUTION; MASS PROTOSTAR; BINARY STARS;
DISKS; PARAMETERS; OUTFLOW; MOTIONS; DUST
AB We present high angular resolution Plateau de Bure Interferometer images (beam of similar to 0 '' 33) of the J = 27. 26 line from several vibrational levels (upsilon(7) = 1 and upsilon(6) = 1) of HC(3)N toward Cepheus A HW2. These images reveal the two main heating sources in the cluster: one centered in the disk collimating the HW2 radio jet (the HW2 disk), and the other associated with a hot core 0 ''.3 northeast HW2 (the HC). This is the first time that vibrationally excited emission of HC3N is spatially resolved in a disk. The kinematics of this emission shows that the HW2 disk rotates following a Keplerian law. We derive the temperature profiles in the two objects from the excitation of HC3N along the HW2 disk and the HC. These profiles reveal that both objects are centrally heated and show temperature gradients. The inner and hotter regions have temperatures of 350 +/- 30 K and 270 +/- 20 K for the HW2 disk and the HC, respectively. In the cooler and outer regions, the temperature drops to 250 +/- 30 K in the HW2 disk, and to 220 +/- 15 K in the HC. The estimated luminosity of the heating source of the HW2 disk is similar to 2.2 x 10(4) L(circle dot), and similar to 3000 L(circle dot) for the HC. The most massive protostar in the HW2 region is the powering source of the HW2 radio jet. We discuss the formation of multiple systems in this cluster. The proximity of the HC to HW2 suggests that these sources likely form a binary system of B stars, explaining the observed precession of the HW2 radio jet.
C1 [Jimenez-Serra, I.; Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Martin-Pintado, J.; Rodriguez-Franco, A.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain.
[Martin, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rodriguez-Franco, A.] Univ Complutense Madrid, Dept Matemat Aplicada Biomatemat, Escuela Univ Opt, E-28037 Madrid, Spain.
[Chandler, C.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Winters, J. M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
RP Jimenez-Serra, I (reprint author), Univ Leeds, Sch Phys & Astron, EC Stoner Bldg, Leeds LS2 9JT, W Yorkshire, England.
EM I.Jimenez-Serra@leeds.ac.uk; jmartin.pintado@iem.cfmac.csic.es;
P.Caselli@leeds.ac.uk; jmartin.pintado@iem.cfmac.csic.es;
arturo@damir.iem.csic.es; cchandle@nrao.edu; winters@iram.fr
RI Martin-Pintado, Jesus/H-6107-2015
OI Martin-Pintado, Jesus/0000-0003-4561-3508
FU Spanish MEC [ESP2004-00665, ESP2007-65812-C02-01]; "Comunidad de Madrid"
Government [S-0505/ESP-0277]
FX We acknowledge the IRAM staff for the support provided during the
observations. We thank two referees for their useful comments that
helped to improve the paper, and W. J. de Wit and E. R. Parkin for
fruitful discussions. J. M. P. acknowledges the Spanish MEC for the
support provided through projects ESP2004-00665, ESP2007-65812-C02-01,
and "Comunidad de Madrid" Government under PRICIT project
S-0505/ESP-0277 (ASTROCAM).
NR 31
TC 12
Z9 12
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2009
VL 703
IS 2
BP L157
EP L161
DI 10.1088/0004-637X/703/2/L157
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 496XV
UT WOS:000270014600014
ER
PT J
AU Winn, JN
Johnson, JA
Albrecht, S
Howard, AW
Marcy, GW
Crossfield, IJ
Holman, MJ
AF Winn, Joshua N.
Johnson, John Asher
Albrecht, Simon
Howard, Andrew W.
Marcy, Geoffrey W.
Crossfield, Ian J.
Holman, Matthew J.
TI HAT-P-7: A RETROGRADE OR POLAR ORBIT, AND A THIRD BODY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; planetary systems: formation; stars: individual
(HAT-P-7); stars: rotation
ID LIGHT-CURVE PROJECT; SPIN-ORBIT; PLANETARY SYSTEM; TRANSIT; STAR;
ALIGNMENT; ROTATION; ECCENTRICITY; MISALIGNMENT; INCLINATION
AB We show that the exoplanet HAT-P-7b has an extremely tilted orbit, with a true angle of at least 86 degrees. with respect to its parent star's equatorial plane, and a strong possibility of retrograde motion. We also report evidence for an additional planet or companion star. The evidence for the unparalleled orbit and the third body is based on precise observations of the star's apparent radial velocity (RV). The anomalous RV due to rotation ( the Rossiter-McLaughlin effect) was found to be a blueshift during the first half of the transit and a redshift during the second half, an inversion of the usual pattern, implying that the angle between the sky-projected orbital and stellar angular momentum vectors is 182 degrees.5 +/- 9 degrees.4. The third body is implicated by excess RV variation of the host star over 2 yr. Some possible explanations for the tilted orbit of HAT-P-7b are a close encounter with another planet, the Kozai effect, and resonant capture by an inward-migrating outer planet.
C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Johnson, John Asher] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Howard, Andrew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Crossfield, Ian J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
RI Howard, Andrew/D-4148-2015
OI Howard, Andrew/0000-0001-8638-0320
FU NSF [AST-0702821]; Netherlands Organisation for Scientific Research
(NWO); NASA [NNX09AD36G, NNX09AB33G]; MIT
FX 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, and was made possible
by the generous financial support of the W. M. Keck Foundation. We
extend special thanks to those of Hawaiian ancestry on whose sacred
mountain of Mauna Kea we are privileged to be guests. Without their
generous hospitality, the Keck observations presented herein would not
have been possible. J.A.J. gratefully acknowledges support from the NSF
Astronomy and Astrophysics Postdoctoral Fellowship program ( grant
AST-0702821). S. A. acknowledges the support of the Netherlands
Organisation for Scientific Research (NWO). J.N.W. gratefully
acknowledges support from the NASA Origins program through awards
NNX09AD36G and NNX09AB33G, and from an MIT Class of 1942 Career
Development Professorship.
NR 39
TC 134
Z9 134
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2009
VL 703
IS 2
BP L99
EP L103
DI 10.1088/0004-637X/703/2/L99
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 496XV
UT WOS:000270014600002
ER
PT J
AU Lilly, SJ
Le Brun, V
Maier, C
Mainieri, V
Mignoli, M
Scodeggio, M
Zamorani, G
Carollo, M
Contini, T
Kneib, JP
Le Fevre, O
Renzini, A
Bardelli, S
Bolzonella, M
Bongiorno, A
Caputi, K
Coppa, G
Cucciati, O
de la Torre, S
de Ravel, L
Franzetti, P
Garilli, B
Iovino, A
Kampczyk, P
Kovac, K
Knobel, C
Lamareille, F
Le Borgne, JF
Pello, R
Peng, YJ
Perez-Montero, E
Ricciardelli, E
Silverman, JD
Tanaka, M
Tasca, L
Tresse, L
Vergani, D
Zucca, E
Ilbert, O
Salvato, M
Oesch, P
Abbas, U
Bottini, D
Capak, P
Cappi, A
Cassata, P
Cimatti, A
Elvis, M
Fumana, M
Guzzo, L
Hasinger, G
Koekemoer, A
Leauthaud, A
Maccagni, D
Marinoni, C
McCracken, H
Memeo, P
Meneux, B
Porciani, C
Pozzetti, L
Sanders, D
Scaramella, R
Scarlata, C
Scoville, N
Shopbell, P
Taniguchi, Y
AF Lilly, Simon J.
Le Brun, Vincent
Maier, Christian
Mainieri, Vincenzo
Mignoli, Marco
Scodeggio, Marco
Zamorani, Gianni
Carollo, Marcella
Contini, Thierry
Kneib, Jean-Paul
Le Fevre, Olivier
Renzini, Alvio
Bardelli, Sandro
Bolzonella, Micol
Bongiorno, Angela
Caputi, Karina
Coppa, Graziano
Cucciati, Olga
de la Torre, Sylvain
de Ravel, Loic
Franzetti, Paolo
Garilli, Bianca
Iovino, Angela
Kampczyk, Pawel
Kovac, Katarina
Knobel, Christian
Lamareille, Fabrice
Le Borgne, Jean-Francois
Pello, Roser
Peng, Yingjie
Perez-Montero, Enrique
Ricciardelli, Elena
Silverman, John D.
Tanaka, Masayuki
Tasca, Lidia
Tresse, Laurence
Vergani, Daniela
Zucca, Elena
Ilbert, Olivier
Salvato, Mara
Oesch, Pascal
Abbas, Umi
Bottini, Dario
Capak, Peter
Cappi, Alberto
Cassata, Paolo
Cimatti, Andrea
Elvis, Martin
Fumana, Marco
Guzzo, Luigi
Hasinger, Gunther
Koekemoer, Anton
Leauthaud, Alexei
Maccagni, Dario
Marinoni, Christian
McCracken, Henry
Memeo, Pierdomenico
Meneux, Baptiste
Porciani, Cristiano
Pozzetti, Lucia
Sanders, David
Scaramella, Roberto
Scarlata, Claudia
Scoville, Nick
Shopbell, Patrick
Taniguchi, Yoshiaki
TI THE zCOSMOS 10k-BRIGHT SPECTROSCOPIC SAMPLE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: active; galaxies: distances and
redshifts; galaxies: evolution; large-scale structure of universe;
quasars: general; surveys
ID ACTIVE GALACTIC NUCLEI; COSMOS FIELD; PHOTOMETRIC REDSHIFT;
STAR-FORMATION; GALAXIES; DENSITY; CATALOG; EVOLUTION; SPECTRA
AB We present spectroscopic redshiftsof a large sample of galaxies with I(AB)< 22.5 in the COSMOS field, measured from spectra of 10,644 objects that have been obtained in the first two years of observations in the zCOSMOS-bright redshift survey. These include a statistically complete subset of 10,109 objects. The average accuracy of individual redshifts is 110 km s(-1), independent of redshift. The reliability of individual redshifts is described by a Confidence Class that has been empirically calibrated through repeat spectroscopic observations of over 600 galaxies. There is very good agreement between spectroscopic and photometric redshifts for the most secure Confidence Classes. For the less secure Confidence Classes, there is a good correspondence between the fraction of objects with a consistent photometric redshift and the spectroscopic repeatability, suggesting that the photometric redshifts can be used to indicate which of the less secure spectroscopic redshifts are likely right and which are probably wrong, and to give an indication of the nature of objects for which we failed to determine a redshift. Using this approach, we can construct a spectroscopic sample that is 99% reliable and which is 88% complete in the sample as a whole, and 95% complete in the redshift range 0.5 < z < 0.8. The luminosity and mass completeness levels of the zCOSMOS-bright sample of galaxies is also discussed.
C1 [Lilly, Simon J.; Maier, Christian; Carollo, Marcella; Caputi, Karina; Kampczyk, Pawel; Kovac, Katarina; Knobel, Christian; Peng, Yingjie; Silverman, John D.; Oesch, Pascal; Porciani, Cristiano] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Le Brun, Vincent; Kneib, Jean-Paul; Le Fevre, Olivier; de la Torre, Sylvain; de Ravel, Loic; Tasca, Lidia; Tresse, Laurence; Abbas, Umi; Cassata, Paolo] Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Mainieri, Vincenzo; Tanaka, Masayuki] European So Observ, D-85748 Garching, Germany.
[Mignoli, Marco; Zamorani, Gianni; Bardelli, Sandro; Bolzonella, Micol; Coppa, Graziano; Cappi, Alberto; Pozzetti, Lucia] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Scodeggio, Marco; Franzetti, Paolo; Garilli, Bianca; Bottini, Dario; Fumana, Marco; Maccagni, Dario; Memeo, Pierdomenico] INAF IASF Milano, I-20133 Milan, Italy.
[Contini, Thierry; Lamareille, Fabrice; Le Borgne, Jean-Francois; Pello, Roser; Perez-Montero, Enrique] Univ Toulouse, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France.
[Renzini, Alvio; Ricciardelli, Elena] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Bongiorno, Angela; Hasinger, Gunther; Meneux, Baptiste] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Iovino, Angela; Guzzo, Luigi] Osserv Astron Brera, INAF, I-20121 Milan, Italy.
[Ilbert, Olivier; Sanders, David] Univ Hawaii, Honolulu, HI 96822 USA.
[Salvato, Mara; Capak, Peter; Cimatti, Andrea; Scarlata, Claudia; Scoville, Nick; Shopbell, Patrick] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Leauthaud, Alexei] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Marinoni, Christian; McCracken, Henry] Ctr Phys Theor, F-13288 Marseille 9, France.
Univ Paris 06, Inst Astrophys Paris, UMR7095, CNRS, F-75014 Paris, France.
[Scaramella, Roberto] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Taniguchi, Yoshiaki] Ehime Univ, Matsuyama, Ehime 7908577, Japan.
RP Lilly, SJ (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
RI Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011; Kneib,
Jean-Paul/A-7919-2015; Mignoli, Marco/O-9426-2015; Cappi,
Alberto/O-9391-2015; Bolzonella, Micol/O-9495-2015; Zucca,
Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015;
OI Iovino, Angela/0000-0001-6958-0304; bottini, dario/0000-0001-6917-041X;
Pozzetti, Lucia/0000-0001-7085-0412; Bongiorno,
Angela/0000-0002-0101-6624; Scodeggio, Marco/0000-0002-2282-5850;
Franzetti, Paolo/0000-0002-6986-0127; Vergani,
Daniela/0000-0003-0898-2216; Scaramella, Roberto/0000-0003-2229-193X;
Oesch, Pascal/0000-0001-5851-6649; Kneib, Jean-Paul/0000-0002-4616-4989;
Mignoli, Marco/0000-0002-9087-2835; Cappi, Alberto/0000-0002-9200-7167;
Bolzonella, Micol/0000-0003-3278-4607; Zucca, Elena/0000-0002-5845-8132;
Bardelli, Sandro/0000-0002-8900-0298; Fumana, Marco/0000-0001-6787-5950;
Maier, Christian/0000-0001-6405-2182; Garilli,
Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X;
Koekemoer, Anton/0000-0002-6610-2048; Perez Montero,
E/0000-0003-3985-4882
FU European Southern Observatory (ESO) Very Large Telescope (VLT) [175];
NASA/ESA Hubble Space Telescope [NAS 5-26555]; National Astronomical
Observatory of Japan; National Research Council of Canada
FX Based on observations undertaken at the European Southern Observatory
(ESO) Very Large Telescope (VLT) under Large Program 175. A-0839. Also
based on observations with the NASA/ESA Hubble Space Telescope, obtained
at the Space Telescope Science Institute, operated by AURA Inc., under
NASA contract NAS 5-26555, with the Subaru Telescope, operated by the
National Astronomical Observatory of Japan, with the telescopes of the
National Optical Astronomy Observatory, operated by the Association of
Universities for Research in Astronomy, Inc. (AURA) under cooperative
agreement with the National Science Foundation, and with the Canada
-France -Hawaii Telescope, operated by the National Research Council of
Canada, the Centre National de la Recherche Scientifique de France, and
the University of Hawaii.
NR 34
TC 257
Z9 257
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD OCT
PY 2009
VL 184
IS 2
BP 218
EP 229
DI 10.1088/0067-0049/184/2/218
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 501NF
UT WOS:000270387900002
ER
PT J
AU Beuther, H
Walsh, AJ
Longmore, SN
AF Beuther, H.
Walsh, A. J.
Longmore, S. N.
TI HOT HIGH-MASS ACCRETION DISK CANDIDATES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: kinematics and dynamics; stars: early-type; stars: formation;
stars: individual (G305.21+0.21, G316.81-0.06, G323.74-0.26, G327.3-0.6,
G328.81+0.63, G331.28-0.19, G336.02-0.83, G345.00-0.22, G351.77-0.54,
G0.55-0.85, G19.47-0.17, IRAS 18151-1208); stars: rotation; techniques:
interferometric
ID HYPERCOMPACT HII-REGIONS; STAR-FORMING-REGIONS; H-II REGIONS; METHANOL
MASERS; MOLECULAR CORES; LINE EMISSION; YOUNG STARS; AMMONIA; OUTFLOWS;
FRAGMENTATION
AB To better understand the physical properties of accretion disks in high-mass star formation, we present a study of a dozen high-mass accretion disk candidates observed at high spatial resolution with the Australia Telescope Compact Array (ATCA) in the high-excitation (4,4) and (5,5) lines of NH(3). All of our originally selected sources were detected in both NH(3) transitions, directly associated with CH(3)OH Class II maser emission and implying that high-excitation NH(3) lines are good tracers of the dense gas components in hot-core-type targets. Only the one source that did not satisfy the initial selection criteria remained undetected. From the 11 mapped sources, six show clear signatures of rotation and/or infall motions. These signatures vary from velocity gradients perpendicular to the outflows, to infall signatures in absorption against ultracompact H II regions, to more spherical infall signatures in emission. Although our spatial resolution is similar to 1000 AU, we do not find clear Keplerian signatures in any of the sources. Furthermore, we also do not find flattened structures. In contrast to this, in several of the sources with rotational signatures, the spatial structure is approximately spherical with sizes exceeding 104 AU, showing considerable clumpy sub-structure at even smaller scales. This implies that on average typical Keplerian accretion disks-if they exist as expected-should be confined to regions usually smaller than 1000 AU. It is likely that these disks are fed by the larger-scale rotating envelope structure we observe here. Furthermore, we do detect 1.25 cm continuum emission in most fields of view. While in some cases weak cm continuum emission is associated with our targets, more typically larger-scale H II regions are seen offset more than 10 '' from our sources. While these H II regions are unlikely to be directly related to the target regions, this spatial association nevertheless additionally stresses that high-mass star formation rarely proceeds in an isolated fashion but in a clustered mode.
C1 [Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Walsh, A. J.] James Cook Univ, Ctr Astron, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia.
[Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Beuther, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM beuther@mpia.de
RI Walsh, Andrew/B-5627-2013
OI Walsh, Andrew/0000-0001-9506-0855
FU Commonwealth of Australia; Deutsche Forschungsgemeinschaft [BE2578]
FX The Australia Telescope Compact Array is part of the Australia Telescope
which is funded by the Commonwealth of Australia for operation as a
National Facility managed by CSIRO. H. B. acknowledges financial support
by the EmmyNoether-Program of the Deutsche Forschungsgemeinschaft (DFG,
grant BE2578).
NR 59
TC 25
Z9 25
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD OCT
PY 2009
VL 184
IS 2
BP 366
EP 386
DI 10.1088/0067-0049/184/2/366
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 501NF
UT WOS:000270387900011
ER
PT J
AU Ahlering, MA
Johnson, DH
Faaborg, J
AF Ahlering, Marissa A.
Johnson, Douglas H.
Faaborg, John
TI FACTORS ASSOCIATED WITH ARRIVAL DENSITIES OF GRASSHOPPER SPARROW
(AMMODRAMUS SAVANNARUM) AND BAIRD'S SPARROW (A. BAIRDII) IN THE UPPER
GREAT PLAINS
SO AUK
LA English
DT Article
DE Ammodramus bairdii; A. savannarum; Baird's Sparrow; Grasshopper Sparrow;
habitat selection; North Dakota; Saskatchewan
ID GRASSLAND BIRDS; SOUTHERN SASKATCHEWAN; TALLGRASS PRAIRIE; HABITAT
ASSOCIATIONS; NORTH-DAKOTA; VEGETATION; SONGBIRDS; AREA; PREDATORS;
SELECTION
AB Although critical to habitat and population management, the proximate cues that birds use to establish territories are largely unknown. Understanding these cues is important for birds, such as many grassland birds, that exhibit high annual variability in population density and make new habitat-selection decisions annually. Identifying the actual cues used is difficult in the field, but the factors associated with the arrival densities of birds can help uncover variables that are involved in or correlated with cues used for selection. During the summers of 2002-2004, we investigated how weather and local vegetation factors were related to arrival densities of Grasshopper Sparrows (Ammodramus savannarum) and Baird's Sparrows (A. bairdii) at three locations across North Dakota and Saskatchewan. Spring densities of Grasshopper Sparrows were positively correlated with concurrent May precipitation, whereas densities of Baird's Sparrows were negatively correlated with the previous winter's snowfall. We used a model-selection approach to evaluate the vegetation characteristics associated with arrival densities of birds. Grasshopper Sparrow densities showed a strong negative relationship to woody cover, and Baird's Sparrow densities showed a negative relationship to vegetation height and vegetation density near the ground. Our results provide a first detailed look at habitat and weather associations immediately after arrival in spring and an important first step in uncovering factors that may be involved in habitat selection in two grassland species. Received 13 August 2008, accepted 20 April 2009.
C1 [Ahlering, Marissa A.; Faaborg, John] Univ Missouri, Columbia, MO 65211 USA.
[Johnson, Douglas H.] US Geol Survey, No Prairie Wildlife Res Ctr, St Paul, MN 55108 USA.
RP Ahlering, MA (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
EM ahleringm@si.edu
FU USGS Northern Prairie Wildlife Research Center, Jamestown, North Dakota
FX We thank the staff at the U.S. Geological Survey (USGS) Northern Prairie
Wildlife Research Center for logistical support and assistance. We are
grateful to the staffs at Chase Lake National Wildlife Refuge (NWR),
Lostwood NWR, the North Dakota Game and Fish Department, The Nature
Conservancy, Ducks Unlimited, and Agriculture Canada (Prairie Farm
Rehabilitation Act) for additional support, assistance, and access to
land. We are also grateful to Lostwood NWR for housing and vehicle
support on the refuge for three years and to the Saskatchewan Watershed
Authority, especially G. McMaster, for help in leasing vehicles. Special
thanks to the field crew; data collection would not have been possible
without them. Thanks to W. A. Cox, R. Hirsh-Jacobson, C. Merkord, M. S.
Pruett, J. Reidy, C. Rittenhouse, M. Ryan, and W. Wehtje for reviewing
the manuscript. This study was funded by the USGS Northern Prairie
Wildlife Research Center, Jamestown, North Dakota, and all banding and
nest-searching protocols were approved by the University of Missouri
Animal Care and Use Committee (no. 3843).
NR 52
TC 6
Z9 6
U1 1
U2 22
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
J9 AUK
JI AUK
PD OCT
PY 2009
VL 126
IS 4
BP 799
EP 808
DI 10.1525/auk.2009.08154
PG 10
WC Ornithology
SC Zoology
GA 508TL
UT WOS:000270959100007
ER
PT J
AU James, HF
AF James, Helen F.
TI REPEATED EVOLUTION OF FUSED THORACIC VERTEBRAE IN SONGBIRDS
SO AUK
LA English
DT Article
DE convergent evolution; notarium; oscine; osteology; Passeri; synsacrum
ID MOLECULAR PHYLOGENY; DARWINS FINCHES; AVIAN RADIATION; AXIAL SKELETON;
AVES; PASSERIFORMES; PATTERNS; PARIDAE
AB The fusion of two or more thoracic vertebrae, independent of the synsacrum, is more widespread in the Passeriformes than has previously been reported. The bone thus formed is known as a "notarium." I surveyed oscine passerine skeletons and found a notarium with fully fused vertebrae in Chabert's Vanga (Leptopterus chabert), certain woodswallows (Artamidae) and shrikes (Laniidae), the Willie Wagtail (Rhipiduridae, Rhipidura leucophrys), the Phainopepla (Bombycillidae, Phainopepla nitens), the penduline tits (Remizidae) including the Verdin (Auriparus flaviceps), various larks (Alaudidae), the Common Starling (Sturnus vulgaris), the sickle-billed thrashers (Toxostoma spp.), and the crossbills (Loxia spp.). Mapping of character evolution on a supertree suggests that a fully fused notarium has evolved independently at least 12 times in the oscine passerines and that notaria with less extensive fusion of the vertebrae (only the spinous processes fused, for example) are even more widespread phylogenetically. Phenotypic expression of a notarium is fixed in some species and higher taxonomic groups but varies within the species in others. Ontogenetically, the fully fused notarium forms when the bird is immature. The evolutionary development of notaria probably depends on mutations that alter expression patterns of transcription genes (Pax and Hox genes are likely candidates) that control embryological differentiation of the vertebrae. Among the systematic implications of this study are additional support for placement of the Verdin in the Remizidae and for the monophyly of a group of western thrashers (Toxostoma spp.) with strongly decurved bills. Received 2 October 2008, accepted 3 May 2009.
C1 Smithsonian Inst, Natl Museum Nat Hist, MRC 116, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP James, HF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 116, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA.
EM jamesh@si.edu
NR 31
TC 3
Z9 4
U1 2
U2 9
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
J9 AUK
JI AUK
PD OCT
PY 2009
VL 126
IS 4
BP 862
EP 872
DI 10.1525/auk.2009.08194
PG 11
WC Ornithology
SC Zoology
GA 508TL
UT WOS:000270959100014
ER
PT J
AU Wunder, MB
Hobson, KA
Kelly, J
Marra, PP
Wassenaar, LI
Stricker, CA
Doucett, RR
AF Wunder, Michael B.
Hobson, Keith A.
Kelly, Jeff
Marra, Peter P.
Wassenaar, Leonard I.
Stricker, Craig A.
Doucett, Richard R.
TI Does a lack of design and repeatability compromise scientific criticism?
A response to Smith et al. (2009).
SO AUK
LA English
DT Letter
ID HYDROGEN ISOTOPE VALUES; STABLE-HYDROGEN; GEOGRAPHIC ASSIGNMENT;
COMPARATIVE EQUILIBRATION; ANIMAL MIGRATION; RAPTOR FEATHERS; ORIGIN;
RATIOS
C1 [Hobson, Keith A.; Wassenaar, Leonard I.] Environm Canada, Saskatoon, SK S7N 3H5, Canada.
[Wunder, Michael B.] Univ Colorado Denver, Dept Biol, Denver, CO 80217 USA.
[Kelly, Jeff] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73072 USA.
[Kelly, Jeff] Univ Oklahoma, Dept Zool, Norman, OK 73072 USA.
[Marra, Peter P.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
[Stricker, Craig A.] US Geol Survey, Denver Fed Ctr, Lakewood, CO 80225 USA.
[Doucett, Richard R.] No Arizona Univ, Colorado Plateau Stable Isotope Lab, Flagstaff, AZ 86011 USA.
RP Hobson, KA (reprint author), Environm Canada, 11 Innovat Blvd, Saskatoon, SK S7N 3H5, Canada.
EM keith.hobson@ec.gc.ca
RI Wassenaar, Leonard/B-7508-2009; Wassenaar, Leonard/B-5996-2013
NR 18
TC 9
Z9 10
U1 2
U2 9
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
EI 1938-4254
J9 AUK
JI AUK
PD OCT
PY 2009
VL 126
IS 4
BP 922
EP 926
PG 5
WC Ornithology
SC Zoology
GA 508TL
UT WOS:000270959100020
ER
PT J
AU Dick, CW
Kress, WJ
AF Dick, Christopher W.
Kress, W. John
TI Dissecting Tropical Plant Diversity with Forest Plots and a Molecular
Toolkit
SO BIOSCIENCE
LA English
DT Article
DE DNA barcoding; tropical forests; community ecology; phylogeny; taxonomy
ID RAIN-FOREST; PHYLOGENETIC STRUCTURE; DNA BARCODES; LAND PLANTS; TREE;
BIODIVERSITY; COMMUNITIES; PATTERNS; AMAZON; DIVERSIFICATION
AB Tropical rainforests are the most biologically diverse of terrestrial bionics. Despite the ecological importance and economic potential of tropical trees, a large fraction of tropical forest tree species lack scientific names, and hundreds of woody plant species in the most intensively studied forest plots remain unidentified. DNA diagnostic tools, including plastid "DNA barcodes" and nuiltilocus genomic markers, can be applied to tropical forest dynamics plots to facilitate taxonomic discovery, Such genetic surveys, as outlined in this article, require expanded herbarium infrastructure and linkages infield ecology, population genetics, and bioinformatics. The fusion of traditional' botany and molecular methods will provide baseline data for understanding both the origin and maintenance of tropical plant diversity.
C1 [Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA.
[Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
[Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Kress, W. John] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Yunnan, Peoples R China.
RP Dick, CW (reprint author), Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA.
EM cwdick@umich.edu; kress@si.edu
RI Dick, Christopher/A-8744-2008
FU National Science Foundation [DEB 043665]
FX Bill Laurance first suggested that we prepare this article. We would
like to thank Mailyn Gonzalez and Jerome Chave for providing information
on the BRIDGE project, the TROPIBIO seminar group at the University of
Michigan for fruitful discussion, and Brian Sedio and Ida Lopez for help
with some of the figures. Paul Berry, Toby Pennington, David Erickson,
and Paul Fine provided useful comments on the manuscript. The authors
thank the Center for Tropical Forest Science (CTFS) and the Smithsonian
Tropical Research Institute for the invitation to participate in a
workshop on evolutionary processes in the CTFS network of plots. C. W.
D. acknowledges the support of the National Science Foundation (DEB
043665).
NR 74
TC 10
Z9 14
U1 2
U2 18
PU AMER INST BIOLOGICAL SCI
PI WASHINGTON
PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA
SN 0006-3568
J9 BIOSCIENCE
JI Bioscience
PD OCT
PY 2009
VL 59
IS 9
BP 745
EP 755
DI 10.1525/bio.2009.59.9.6
PG 11
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 504RK
UT WOS:000270634700006
ER
PT J
AU Figueiredo, E
Soares, M
Seibert, G
Smith, GF
Faden, RB
AF Figueiredo, E.
Soares, M.
Seibert, G.
Smith, G. F.
Faden, R. B.
TI The botany of the Cunene-Zambezi Expedition with notes on Hugo Baum
(1867-1950)
SO BOTHALIA
LA English
DT Article
DE Angola; Baum; collectors; flora
AB A record and discussion of the Cunene-Zambezi Expedition that took place in Angola from 1899 to 1900 is provided. Although the main aim of the expedition was to evaluate the economic potential of southern Angola, it also resulted in significant botanical collections made by Hugo Baum (1867-1950), many of which serve as holotypes of names of plants from the region, and beyond. The itinerary is supplemented by a map illustrating the route followed by the expedition, and locality names are clarified and updated. A full list of the type specimens of flowering plants is provided, with their nomenclature updated and an indication of where known duplicates are housed.
C1 [Figueiredo, E.; Smith, G. F.] Univ Pretoria, Dept Bot, HGWJ Schweickerdt Herbarium, Acocks Chair, ZA-0002 Pretoria, South Africa.
[Soares, M.] Univ Coimbra, Dept Bot, P-3001455 Coimbra, Portugal.
[Seibert, G.] CEA, ISCTE, Lisbon, Portugal.
[Smith, G. F.] S African Natl Biodivers Inst, ZA-0001 Pretoria, South Africa.
[Faden, R. B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
RP Figueiredo, E (reprint author), Univ Pretoria, Dept Bot, HGWJ Schweickerdt Herbarium, Acocks Chair, ZA-0002 Pretoria, South Africa.
EM estrelafigueiredo@hotmail.com; miguel.vonberg@gmail.com;
mailseibert@yahoo.com; smithg@sanbi.org; fadenr@si.edu
OI Figueiredo, Estrela/0000-0002-8511-8213
NR 66
TC 1
Z9 2
U1 0
U2 2
PU NATL BOTANICAL INST
PI PRETORIA
PA PRIVATE BAG X101, PRETORIA 0001, SOUTH AFRICA
SN 0006-8241
J9 BOTHALIA
JI Bothalia
PD OCT
PY 2009
VL 39
IS 2
BP 185
EP 211
PG 27
WC Plant Sciences
SC Plant Sciences
GA 574GO
UT WOS:000275977600005
ER
PT J
AU Zeder, MA
Smith, BD
AF Zeder, Melinda A.
Smith, Bruce D.
TI A Conversation on Agricultural Origins Talking Past Each Other in a
Crowded Room
SO CURRENT ANTHROPOLOGY
LA English
DT Editorial Material
ID EASTERN NORTH-AMERICA; NEAR-EAST; SOUTHERN LEVANT; DOMESTICATION;
TRANSITION; HOLOCENE; PLANT; CULTIVATION; PLEISTOCENE; HUSBANDRY
C1 [Zeder, Melinda A.; Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20013 USA.
RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, POB 37012, Washington, DC 20013 USA.
EM zederm@si.edu
NR 73
TC 36
Z9 37
U1 5
U2 22
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0011-3204
J9 CURR ANTHROPOL
JI Curr. Anthropol.
PD OCT
PY 2009
VL 50
IS 5
BP 681
EP 691
DI 10.1086/605553
PG 11
WC Anthropology
SC Anthropology
GA 493TC
UT WOS:000269759900018
ER
PT J
AU Myers, JA
Harms, KE
AF Myers, Jonathan A.
Harms, Kyle E.
TI Local immigration, competition from dominant guilds, and the ecological
assembly of high-diversity pine savannas
SO ECOLOGY
LA English
DT Article
DE biodiversity; bunchgrass; community assembly; dispersal assembly;
dominant guild; local immigration; longleaf pine savanna; niche
assembly; recruitment limitation; shrub; species coexistence;
species-rich community
ID RECRUITMENT LIMITATION; COMMUNITY ECOLOGY; SPECIES RICHNESS; PLANT;
GRASSLAND; NICHE; COEXISTENCE; MECHANISMS; NEUTRALITY; DISPERSAL
AB In high-diversity communities, rare species encounter one another infrequently and therefore may compete more intensely with common species or guilds for limiting space and resources. In addition, rare species may be strongly recruitment limited because of their low abundances. Under these conditions, stochastic dispersal and immigration history can have an important influence on community structure. We tested the hypothesis that local immigration and competition from common, large-stature guilds interact to structure local biodiversity in high-diversity longleaf pine savanna groundcover assemblages (> 30 species/m(2)). In two factorial field experiments, we increased local immigration by adding seeds of 38 mostly rare, small-stature forbs and sedges to plots physically dominated by either a common, large-stature bunchgrass or shrub species and to plots in which competition from these dominant guilds was reduced. We measured species richness and abundance at two spatial scales (0.01 and 0.25 m(2)) over two years. Immigration increased total species richness and richness of focal seed addition species regardless of levels of competition with bunchgrasses and shrubs, indicating that many rare, small-stature species can recruit in the face of potential competition from dominant guilds. Removal of dominant guilds increased total and focal species richness in shrub-dominated but not bunchgrass-dominated plots. In addition, competition from both dominant guilds had no clear effect on rank-abundance distributions of focal species. Our results suggest a key role for dispersal assembly in structuring local biodiversity in this high-diversity plant community, but the importance of this mechanism depends on the strength of local niche assembly involving competition from some, but not all, dominant guilds.
C1 [Myers, Jonathan A.; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Div Systemat Ecol & Evolut, Baton Rouge, LA 70803 USA.
[Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Myers, JA (reprint author), Louisiana State Univ, Dept Biol Sci, Div Systemat Ecol & Evolut, Baton Rouge, LA 70803 USA.
EM jmyer19@lsu.edu
FU Louisiana State University; Louisiana Office of Environmental Education;
National Science Foundation
FX Financial support was provided by a Torrey Botanical Society graduate
student fellowship, Sigma-Xi Grant-In-Aid (Louisiana State University
Chapter), Louisiana Office of Environmental Education grants, and the
National Science Foundation.
NR 56
TC 30
Z9 30
U1 2
U2 29
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
J9 ECOLOGY
JI Ecology
PD OCT
PY 2009
VL 90
IS 10
BP 2745
EP 2754
DI 10.1890/08-1953.1
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 500CH
UT WOS:000270274200011
PM 19886484
ER
PT J
AU Comita, LS
Engelbrecht, BMJ
AF Comita, Liza S.
Engelbrecht, Bettina M. J.
TI Seasonal and spatial variation in water availability drive habitat
associations in a tropical forest
SO ECOLOGY
LA English
DT Article
DE Barro Colorado Island, Panama; drought; Forest Dynamics Plot; niche
differentiation; species distributions
ID TREE SPECIES DISTRIBUTIONS; BORNEAN RAIN-FOREST; EL-NINO; NEOTROPICAL
FOREST; SEEDLING DYNAMICS; SOIL NUTRIENTS; BETA-DIVERSITY; SEVERE
DROUGHT; DRY SEASON; GROWTH
AB Associations with topographic units or soil types that vary in water availability are widespread in plant communities and are one of the main structuring aspects for local species distribution patterns, yet the underlying mechanisms are poorly understood. We hypothesized that differential seedling performance across habitats, particularly during the dry season, leads to habitat associations in seasonal tropical forests. We expected this pattern to be most pronounced in particularly dry years, such as those associated with El Nino Southern Oscillation (ENSO) events. We assessed performance of 36 native tree and shrub species in a moist forest in central Panama across the dry and wet seasons in two topographic habitat types during a year in which dry-season precipitation was reduced due to an ENSO event. At the community level, we found lower growth and higher mortality in the dry season relative to the wet season and higher mortality in the drier plateau habitat relative to the wetter slope habitat. There was large variation in species' responses to season and habitat. Species' mortality and growth rates were significantly correlated with experimentally assessed drought sensitivity, but only during the dry season in the plateau habitat. Slope specialists had significantly higher survival, but not growth, in the slope vs. plateau habitat during the dry season. In contrast, plateau specialists showed no performance differences between habitats. The data suggest that associations with plateau habitats result from a numerical advantage of drought-tolerant species in dry habitats in which seedlings of drought-sensitive species are unable to persist. Overall, our results support the idea that seasonal and spatial variation in water availability, particularly in dry years, drive seedling dynamics, which in turn shape local species distributions. Predicted shifts in rainfall patterns caused by global and regional climate change are therefore expected to alter the dynamics, composition, and diversity of seasonal tropical forests.
C1 [Comita, Liza S.] Univ Georgia, Dept Plant Biol, Athens, GA 30606 USA.
[Engelbrecht, Bettina M. J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Comita, LS (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
EM lsc2125@columbia.edu
RI Engelbrecht, Bettina/E-9914-2012
FU Center for Tropical Forest Sciences (CTFS); Smithsonian Tropical
Research Institute; U. S. National Science Foundation [DEB-0075102]; NSF
Graduate Research Fellowship and University of Georgia Presidential
Fellowship; German Research Foundation (DFG)
FX This study was funded by a grant from the Center for Tropical Forest
Sciences (CTFS) at the Smithsonian Tropical Research Institute.
Additional funding was provided by the U. S. National Science Foundation
(DEB-0075102). L. S. Comita acknowledges the support of an NSF Graduate
Research Fellowship and University of Georgia Presidential Fellowship,
and B. M. J. Engelbrecht was supported by the German Research Foundation
(DFG). Valuable comments on the manuscript were provided by G.
Goldsmith, C. E. T. Paine, and three anonymous reviewers.
NR 66
TC 72
Z9 79
U1 7
U2 71
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD OCT
PY 2009
VL 90
IS 10
BP 2755
EP 2765
DI 10.1890/08-1482.1
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 500CH
UT WOS:000270274200012
PM 19886485
ER
PT J
AU Marra, PP
Dove, C
Dolbeer, R
AF Marra, Peter P.
Dove, Carla
Dolbeer, Richard
TI Birdstrikes: a reply to Swift et al.
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Letter
C1 [Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC USA.
[Dove, Carla] Smithsonian Inst, Natl Museum Nat Hist, Feather Identificat Lab, Washington, DC 20560 USA.
[Dolbeer, Richard] Wildlife Serv, USDA, Sandusky, OH USA.
RP Marra, PP (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC USA.
EM marrap@si.edu
NR 3
TC 1
Z9 1
U1 1
U2 4
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1540-9295
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD OCT
PY 2009
VL 7
IS 8
BP 407
EP 408
DI 10.1890/09.WB.026
PG 3
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 508RD
UT WOS:000270949800013
ER
PT J
AU Buzas, MA
Culver, SJ
AF Buzas, Martin A.
Culver, Stephen J.
TI Geographic origin of species: The temperate-tropical interchange
SO GEOLOGY
LA English
DT Article
ID BENTHIC FORAMINIFERA; DIVERSITY; DISPERSAL
AB The tropics are often evoked as a center for species origination. Foraminifera are one of the few groups of organisms with a fossil record sufficient to establish the geographic origin of species. The modern foraminiferal biota on the Atlantic continental margin of North America contains 259 species with a fossil record. The worldwide geographic origin of these species was documented using museum collections. Only 14% of these species originated in the subpolar regions, whereas nearly equal proportions originated in the temperate regions (46%) and tropical regions (40%). Moreover, the majority (76%) of species originating in the temperate regions now also occur in the modern tropical biota. These foraminiferal data suggest that, in contrast to the center of origin hypothesis, the biota of temperate and tropical latitudes act in concert with a substantial species interchange between them.
C1 [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist MRC 121, Washington, DC 20013 USA.
[Culver, Stephen J.] E Carolina Univ, Dept Geol, Greenville, NC 27858 USA.
RP Buzas, MA (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist MRC 121, Washington, DC 20013 USA.
EM buzasm@si.edu; culvers@ecu.edu
NR 19
TC 6
Z9 6
U1 0
U2 7
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD OCT
PY 2009
VL 37
IS 10
BP 879
EP 881
DI 10.1130/G30287A.1
PG 3
WC Geology
SC Geology
GA 501MV
UT WOS:000270386900004
ER
PT J
AU Falcon-Lang, HJ
Nelson, WJ
Elrick, S
Looy, CV
Ames, PR
DiMichele, WA
AF Falcon-Lang, Howard J.
Nelson, W. John
Elrick, Scott
Looy, Cindy V.
Ames, Philip R.
DiMichele, William A.
TI Incised channel fills containing conifers indicate that seasonally dry
vegetation dominated Pennsylvanian tropical lowlands
SO GEOLOGY
LA English
DT Article
ID CLIMATE; CYCLOTHEMS; FOREST; MODEL; USA
AB The idea that the Pennsylvanian tropical lowlands were temporally dominated by rainforest (i.e., the Coal Forest) is deeply ingrained in the literature. Here we challenge two centuries of research by suggesting that this concept is based on a taphonomic artifact, and that seasonally dry vegetation dominated instead. This controversial finding arises from the discovery of a new middle Pennsylvanian (Moscovian) fossil plant assemblage in southeast Illinois, United States. The assemblage, which contains xerophytic walchian conifers, occurs in channels incised into a calcic Vertisol below the Baker Coal. These plants grew on seasonally dry tropical lowlands inferred to have developed during a glacial phase. This xerophytic flora differs markedly from that of the typical clubmoss-dominated Coal Forest developed during deglaciation events. Although preserved only very rarely, we argue that such xerophytic floras were temporally as dominant, and perhaps more dominant, than the iconic Coal Forests, which are overrepresented in the fossil record due to taphonomic megabias. These findings require the iconography of Pennsylvanian tropical lowlands to be redrawn.
C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England.
[Nelson, W. John; Elrick, Scott] Illinois State Geol Survey, Champaign, IL 61820 USA.
[Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Ames, Philip R.] Peabody Energy, Evansville, IN 47715 USA.
[DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England.
EM h.falcon-lang@es.rhul.ac.uk
RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012
FU Natural Environment Research Council Advanced Postdoctoral Fellowship
[NE/F014120/2]
FX We thank Peabody Energy for allowing access to the Cottage Grove Mine,
and David Williams (Kentucky Geological Survey) for sharing data.
Falcon-Lang acknowledges a Natural Environment Research Council Advanced
Postdoctoral Fellowship (NE/F014120/2).
NR 18
TC 62
Z9 64
U1 0
U2 10
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD OCT
PY 2009
VL 37
IS 10
BP 923
EP 926
DI 10.1130/G30117A.1
PG 4
WC Geology
SC Geology
GA 501MV
UT WOS:000270386900016
ER
PT J
AU Gloor, M
Phillips, OL
Lloyd, JJ
Lewis, SL
Malhi, Y
Baker, TR
Lopez-Gonzalez, G
Peacock, J
Almeida, S
de Oliveira, ACA
Alvarez, E
Amaral, I
Arroyo, L
Aymard, G
Banki, O
Blanc, L
Bonal, D
Brando, P
Chao, KJ
Chave, J
Davila, N
Erwin, T
Silva, J
Di Fiore, A
Feldpausch, TR
Freitas, A
Herrera, R
Higuchi, N
Honorio, E
Jimenez, E
Killeen, T
Laurance, W
Mendoza, C
Monteagudo, A
Andrade, A
Neill, D
Nepstad, D
Vargas, PN
Penuela, MC
Cruz, AP
Prieto, A
Pitman, N
Quesada, C
Salomao, R
Silveira, M
Schwarz, M
Stropp, J
Ramirez, F
Ramirez, H
Rudas, A
ter Steege, H
Silva, N
Torres, A
Terborgh, J
Vasquez, R
van der Heijden, G
AF Gloor, M.
Phillips, O. L.
Lloyd, J. J.
Lewis, S. L.
Malhi, Y.
Baker, T. R.
Lopez-Gonzalez, G.
Peacock, J.
Almeida, S.
Alves de Oliveira, A. C.
Alvarez, E.
Amaral, I.
Arroyo, L.
Aymard, G.
Banki, O.
Blanc, L.
Bonal, D.
Brando, P.
Chao, K. -J.
Chave, J.
Davila, N.
Erwin, T.
Silva, J.
Di Fiore, A.
Feldpausch, T. R.
Freitas, A.
Herrera, R.
Higuchi, N.
Honorio, E.
Jimenez, E.
Killeen, T.
Laurance, W.
Mendoza, C.
Monteagudo, A.
Andrade, A.
Neill, D.
Nepstad, D.
Nunez Vargas, P.
Penuela, M. C.
Pena Cruz, A.
Prieto, A.
Pitman, N.
Quesada, C.
Salomao, R.
Silveira, Marcos
Schwarz, M.
Stropp, J.
Ramirez, F.
Ramirez, H.
Rudas, A.
ter Steege, H.
Silva, N.
Torres, A.
Terborgh, J.
Vasquez, R.
van der Heijden, G.
TI Does the disturbance hypothesis explain the biomass increase in
basin-wide Amazon forest plot data?
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE Amazon rainforest; carbon sink; disturbance; mortality; power law
ID ATMOSPHERIC CARBON-DIOXIDE; LONG-TERM PLOTS; TROPICAL FORESTS; LARGE
BLOWDOWNS; TURNOVER; DYNAMICS; PATTERNS
AB Positive aboveground biomass trends have been reported from old-growth forests across the Amazon basin and hypothesized to reflect a large-scale response to exterior forcing. The result could, however, be an artefact due to a sampling bias induced by the nature of forest growth dynamics. Here, we characterize statistically the disturbance process in Amazon old-growth forests as recorded in 135 forest plots of the RAINFOR network up to 2006, and other independent research programmes, and explore the consequences of sampling artefacts using a data-based stochastic simulator. Over the observed range of annual aboveground biomass losses, standard statistical tests show that the distribution of biomass losses through mortality follow an exponential or near-identical Weibull probability distribution and not a power law as assumed by others. The simulator was parameterized using both an exponential disturbance probability distribution as well as a mixed exponential-power law distribution to account for potential large-scale blowdown events. In both cases, sampling biases turn out to be too small to explain the gains detected by the extended RAINFOR plot network. This result lends further support to the notion that currently observed biomass gains for intact forests across the Amazon are actually occurring over large scales at the current time, presumably as a response to climate change.
C1 [Gloor, M.; Phillips, O. L.; Lloyd, J. J.; Lewis, S. L.; Baker, T. R.; Lopez-Gonzalez, G.; Peacock, J.; Feldpausch, T. R.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Malhi, Y.] Univ Oxford, Oxford, England.
[Almeida, S.] Paraense Emilio Goeldi, Belem, Para, Brazil.
[Alves de Oliveira, A. C.; Amaral, I.] Team INPA, Manaus, Amazonas, Brazil.
[Alvarez, E.] Columbia Univ, Medellin, Colombia.
[Arroyo, L.] Missouri Bot Garden, Santa Cruz, Bolivia.
[Arroyo, L.] Museo Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia.
[Aymard, G.] UNELLEZ Guanare, Guanare, Venezuela.
[Banki, O.; Stropp, J.] Univ Utrecht, NL-3508 TC Utrecht, Netherlands.
[Blanc, L.; Bonal, D.] UMR, Kourou, French Guiana.
[Erwin, T.] Smithsonian Inst, Washington, DC 20560 USA.
[Silva, J.] Univ San Abad Cusco, Cuzco, Peru.
[Di Fiore, A.] NYU, New York, NY USA.
[Freitas, A.] Museu Paraense Emilio Goeldi, Belem, Para, Brazil.
[Herrera, R.] IVIC, Caracas, Venezuela.
[Higuchi, N.] Inst Natl Pesquisas Amazonia, Manaus, Amazonas, Brazil.
[Honorio, E.] IIAP, Iquitos, Peru.
[Jimenez, E.] Univ Nacl Colombia, Leticia, Colombia.
[Killeen, T.] Conservat Int, Washington, DC USA.
[Laurance, W.] Smithsonian Trop Res Inst, Ancon, Panama.
[Mendoza, C.] Manejo Forestal Tierras Trop Bolivia, Fomabo, Sacta, Bolivia.
[Monteagudo, A.; Pena Cruz, A.; Vasquez, R.] Jardin Bot Missouri, Proyecto Flora Peru, Oxapampa, Peru.
[Andrade, A.] INPA, Manaus, Amazonas, Brazil.
[Neill, D.] Fdn Jatun Sacha, Quito, Ecuador.
[Neill, D.] Missouri Bot Garden, Quito, Ecuador.
[Nepstad, D.] Woods Hole Res Ctr, Woods Hole, MA USA.
[Nunez Vargas, P.] Univ San Antonio Abad Cusco, Cuzco, Peru.
[Penuela, M. C.] Univ Nacl Colombia, Leticia, Amazonas, Brazil.
[Prieto, A.; Rudas, A.] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia.
[Pitman, N.] Duke Univ, Ctr Trop Conservat, Durham, NC 27706 USA.
[Quesada, C.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Salomao, R.] Museu Paraense Emilio Goeldi, Belem, Para, Brazil.
[Silveira, Marcos] Univ Fed Acre, Acre, Brazil.
[Ramirez, F.] Univ Nacl Amazonia Peruana, Iquitos, Peru.
[Ramirez, H.; Torres, A.] Univ Los Andes, Merida, Venezuela.
[ter Steege, H.] NHN Utrecht, Utrecht, Netherlands.
[Silva, N.] CIFOR, Tapajos, Brazil.
[Silva, N.] EMBRAPA Amazonia Oriental, Belem, Para, Brazil.
RP Gloor, M (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
EM eugloor@googlemail.com
RI Lloyd, Jonathan/F-8893-2010; Pitman, Nigel/A-7681-2008; Phillips,
Oliver/A-1523-2011; Brando, Paulo/C-4302-2012; ter Steege,
Amaz/B-5866-2011; Feldpausch, Ted/D-3436-2009; Silveira,
Marcos/H-7906-2013; Honorio Coronado, Euridice/K-3412-2015
OI Lewis, Simon/0000-0002-8066-6851; Lloyd, Jonathan/0000-0002-5458-9960;
Pitman, Nigel/0000-0002-9211-2880; Phillips, Oliver/0000-0002-8993-6168;
Brando, Paulo/0000-0001-8952-7025; ter Steege, Amaz/0000-0002-8738-2659;
Feldpausch, Ted/0000-0002-6631-7962; Silveira,
Marcos/0000-0003-0485-7872; Honorio Coronado,
Euridice/0000-0003-2314-590X
FU Earth and Biosphere Institute (Gloor); Leverhulme Trust (Phillips); NERC
[NE/B503384/1, NE/D01025X/1, NER/A/S/2003/00608/2, WOTRO (W84-581)];
Royal Society; University of Leeds; Gordon and Betty Moore Foundation
FX The results summarized here derive from several grants and contributions
from numerous field assistants and rural communities across Amazonia,
many previously acknowledged. The following assisted with recent
censuses: I. Huamantupa, N. Jaramillo, N. Saavedram (Peru), V. Pena
(Ecuador), J.-C. Arias, D. Navarrete (Colombia). We thank CNPQ (Brazil),
MCT (Brazil), Ministerio del Medio Ambiente, Vivienda y Desarrollo
Territorial (Colombia), Ministerio de Ambiente (Ecuador), the Forestry
Commission (Guyana), INRENA (PerU), and Ministerio del Ambiente para el
Poder Popular (Venezuela) for research permissions. This paper was
supported in particular by the Earth and Biosphere Institute (Gloor),
Leverhulme Trust (Phillips), NERC grants NE/B503384/1 and NE/D01025X/1
(Phillips), NER/A/S/2003/00608/2 (Malhi), WOTRO (W84-581) (ter Steege,
Banki), the Royal Society (Lewis, Malhi), University of Leeds (Baker,
Chao), and a Gordon and Betty Moore Foundation grant to RAINFOR.
Additional data used here were collected with support from the TEAM
Network of Conservation International, funded by the Gordon and Betty
Moore Foundation. We also thank Bruce Nelson for providing the original
data on Amazon forest blow-downs of his 1994 publication. Finally we
thank Aaron Clauset and Cosma Rohilla Shalizi for making their routines
for power law estimation available to us.
NR 25
TC 43
Z9 44
U1 2
U2 41
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD OCT
PY 2009
VL 15
IS 10
BP 2418
EP 2430
DI 10.1111/j.1365-2486.2009.01891.x
PG 13
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 491KO
UT WOS:000269577800006
ER
PT J
AU Campbell, BA
AF Campbell, Bruce A.
TI Scale-Dependent Surface Roughness Behavior and Its Impact on Empirical
Models for Radar Backscatter
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Radar polarimetry; radar scattering; remote sensing
ID BARE SOIL SURFACES; INTEGRAL-EQUATION MODEL; POWER-LAW SPECTRUM;
COHERENT BACKSCATTER; PROFILE LENGTH; SAR DATA; SCATTERING; MOISTURE;
PARAMETERS; COEFFICIENTS
AB One goal of radar remote sensing is the extraction of terrain statistics and surface dielectric properties from backscatter data for some range of wavelengths, incidence angles, and polarizations. This paper addresses empirical approaches used to estimate terrain properties from radar data over a wider range of roughness than permitted by analytical models. Many empirical models assume, at least implicitly, that roughness parameters like rms height or correlation length are independent of the horizontal length scale over which they are measured, in contrast to recent surveys of natural terrain, which show that self-affine, or power-law scaling, between horizontal scale and roughness statistics is very common. The rms slope at the horizontal scale of the illuminating wavelength s(lambda) is directly related to the variogram or structure function of a self-affine surface, can be readily obtained from field-measured topography, and, when used in an empirical model, avoids the need for arbitrary wavelength-dependent terms. To facilitate comparison with earlier approaches, an expression that links the rms height at some profile length with the rms (Allan) deviation at an equivalent horizontal sampling interval is obtained from numerical simulations. An empirical model for polarimetric scattering as a function of s(lambda) at 35 degrees-60 degrees incidence from smooth to rugged lava surfaces is derived and compared with earlier models for backscatter from modestly rough soil surfaces. The asymptotic behavior of polarization ratios for the lava flows suggests that the depolarization of linear-polarized illuminating signals occurs as a first-order process, likely through single scattering by rock edges or other discontinuities, rather than as the solely multiple-scattering effect predicted by some analytical models. Efforts to fully understand radar scattering from geological surfaces need to incorporate wavelength-scale roughness, perhaps through computational simulations.
C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
FU NASA Planetary Geology and Geophysics Program
FX This work was supported in part by a grant from the NASA Planetary
Geology and Geophysics Program.
NR 58
TC 12
Z9 12
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD OCT
PY 2009
VL 47
IS 10
BP 3480
EP 3488
DI 10.1109/TGRS.2009.2022752
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 498JR
UT WOS:000270136200017
ER
PT J
AU Tavzes, C
Silc, F
Kladnik, A
Fackler, K
Messner, K
Pohleven, F
Koestler, RJ
AF Tavzes, Crtomir
Silc, Franc
Kladnik, Andrej
Fackler, Karin
Messner, Kurt
Pohleven, Franc
Koestler, Robert J.
TI Enzymatic degradation of mould stains on paper analysed by colorimetry
and DRIFT-IR spectroscopy
SO INTERNATIONAL BIODETERIORATION & BIODEGRADATION
LA English
DT Article
DE Melanin degradation; White-rot fungi; Laccase; Manganese peroxidase;
FTIR; Colorimetry
ID FUNGAL MELANINS; OXIDATION MECHANISM; NONPHENOLIC LIGNIN; LACCASE;
BIOSYNTHESIS; LIGNOCELLULOSE; MEDIATORS; ENZYMES; SYSTEMS
AB Melanin is chemically and by physical characteristics very similar to lignin, a major constituent of wood, and therefore ligninolytic enzymes of white-rot fungi were tested for their ability to selectively degrade melanin. Melanin degradation was studied both in liquid suspensions of melanin and on melaninised paper samples. Liquid suspension samples were tested for changes in their chemical composition (appearance and relative representation of functional groups and chemical bonds) with FTIR spectrometry. Changes in colour of melaninised paper samples were investigated with a colorimeter. Effectiveness of the treatment (bleaching) was determined as a change in lightness (Delta L). Melanin was oxidised in the liquid suspensions, and the intensity of modification varied depending on the procedure employed. The most pronounced changes in melanin were observed in laccase-1-hydroxybenzotriazole (HBT) treatment at heightened air pressure. The most prominent discoloration of the melaninised paper samples (and no visually detectable damage to the integrity of the paper) was, like in the case of the liquid suspensions, observed after laccase-HBT treatment. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Tavzes, Crtomir] Inst Wood Sci & Technol & Sustainable Dev, SI-1000 Ljubljana, Slovenia.
[Silc, Franc; Kladnik, Andrej; Pohleven, Franc] Univ Ljubljana, Biotech Fac, Dept Wood Sci & Technol, Ljubljana 61000, Slovenia.
[Fackler, Karin; Messner, Kurt] Vienna Univ Technol, Inst Chem Engn, Vienna, Austria.
[Koestler, Robert J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA.
[Tavzes, Crtomir] Inst Protect Cultural Heritage Slovenia, Restorat Ctr, Dept Conservat Sci, Ljubljana, Slovenia.
[Tavzes, Crtomir] Metropolitan Museum Art, Dept Sci Res, New York, NY 10028 USA.
RP Tavzes, C (reprint author), Inst Wood Sci & Technol & Sustainable Dev, Celovska Cesta 268, SI-1000 Ljubljana, Slovenia.
EM crtomir.tavzes@iltra.si
NR 42
TC 8
Z9 8
U1 2
U2 10
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0964-8305
J9 INT BIODETER BIODEGR
JI Int. Biodeterior. Biodegrad.
PD OCT
PY 2009
VL 63
IS 7
BP 873
EP 879
DI 10.1016/j.ibiod.2009.07.001
PG 7
WC Biotechnology & Applied Microbiology; Environmental Sciences
SC Biotechnology & Applied Microbiology; Environmental Sciences & Ecology
GA 513OZ
UT WOS:000271333700010
ER
PT J
AU Green, KC
Armstrong, JS
Soon, W
AF Green, Kesten C.
Armstrong, J. Scott
Soon, Willie
TI Validity of climate change forecasting for public policy decision making
SO INTERNATIONAL JOURNAL OF FORECASTING
LA English
DT Article
DE Climate model; Ex ante forecasts; Out-of-sample errors; Predictability;
Public policy; Relative absolute errors; Unconditional forecasts
AB Policymakers need to know whether prediction is possible and, if so, whether any proposed forecasting method will provide forecasts that are substantially more accurate than those from the relevant benchmark method. An inspection of global temperature data suggests that temperature is subject to irregular variations on all relevant time scales, and that variations during the late 1900s were not unusual. In such a situation, a "no change" extrapolation is an appropriate benchmark forecasting method. We used the UK Met Office Hadley Centre's annual average thermometer data from 1850 through 2007 to examine the performance of the benchmark method. The accuracy of forecasts from the benchmark is such that even perfect forecasts would be unlikely to help policymakers. For example, mean absolute errors for the 20- and 50-year horizons were 0.18 degrees C and 0.24 degrees C respectively. We nevertheless demonstrate the use of benchmarking with the example of the Intergovernmental Panel on Climate Change's 1992 linear projection of long-term warming at a rate of 0.03 degrees C per year. The small sample of errors from ex ante projections at 0.03 degrees C per year for 1992 through 2008 was practically indistinguishable from the benchmark errors. Validation for long-term forecasting, however, requires a much longer horizon. Again using the IPCC warming rate for our demonstration, we projected the rate successively over a period analogous to that envisaged in their scenario of exponential CO(2) growth-the years 1851 to 1975. The errors from the projections were more than seven times greater than the errors from the benchmark method. Relative errors were larger for longer forecast horizons. Our validation exercise illustrates the importance of determining whether it is possible to obtain forecasts that are more useful than those from a simple benchmark before making expensive policy decisions. (C) 2009 International Institute of Forecasters. Published by Elsevier B.V. All rights reserved.
C1 [Green, Kesten C.] Monash Univ, Business & Econ Forecasting, Clayton, Vic 3800, Australia.
[Armstrong, J. Scott] Univ Penn, Wharton Sch, Philadelphia, PA 19104 USA.
[Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Green, KC (reprint author), POB 10800, Wellington 6143, New Zealand.
EM kesten@me.com; armstrong@wharton.upenn.edu; wsoon@cfa.harvard.edu
RI Green, Kesten/F-3716-2013
OI Green, Kesten/0000-0001-9122-885X
NR 9
TC 10
Z9 10
U1 2
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-2070
J9 INT J FORECASTING
JI Int. J. Forecast.
PD OCT-DEC
PY 2009
VL 25
IS 4
BP 826
EP 832
DI 10.1016/j.ijforecast.2009.05.011
PG 7
WC Economics; Management
SC Business & Economics
GA 519CI
UT WOS:000271742200019
ER
PT J
AU Colin, P
Beilicke, M
Davies, F
Harris, DE
Hui, CM
Mazin, D
Raue, M
Wagner, RM
Wagner, S
Walker, RC
AF Colin, Pierre
Beilicke, Matthias
Davies, Frederick
Harris, D. E.
Hui, C. M.
Mazin, Daniel
Raue, Martin
Wagner, R. M.
Wagner, Stefan
Walker, R. C.
CA HESS Collaboration
MAGIC Collaboration
VERITAS Collaboration
Chandra Collaboration
VLBA Collaboration
TI THE 2008 MULTIWAVELENGTH CAMPAIGN OF THE TeV RADIO-GALAXY M87
SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D
LA English
DT Article; Proceedings Paper
CT International Workshop on High-Energy Gamma-Rays and Neutrinos from
Extra-Galactic Sources
CY JAN 13-16, 2009
CL Heidelberg, GERMANY
DE Active galactic nuclei: individual (M87); gamma-rays; X-rays; radio
ID GAMMA-RAY EMISSION; HUBBLE-SPACE-TELESCOPE; JET; DISCOVERY; M-87
AB M87 is the first and brightest radio galaxy detected in the TeV regime. It is the closest extragalactic object showing variability and the only one that does not have its jet pointing toward the line of sight. The structure of the M87 jet is spatially resolved in Xray, optical and radio observations. Time correlation between the TeV flux and emission at other wavelengths provides a unique opportunity to localize the VHE emission process occurring in active galaxy nuclei. For 10 years, M87 has been monitored in the TeV band by imaging air Cherenkov telescopes (IACT) as well as in X-ray, optical and radio bands. In 2008, the three main IACTs, H.E.S.S./MAGIC/VERITAS, coordinated their observations in a joint campaign. In February, high TeV activities with rapid flares have been detected. Contemporaneously, M87 was observed with high resolution instruments in the X-ray (Chandra) and Radio band (VLBA).
C1 [Colin, Pierre; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Beilicke, Matthias] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Davies, Frederick; Walker, R. C.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Harris, D. E.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Hui, C. M.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA.
[Mazin, Daniel] Univ Autonoma Barcelona, IFAE, Bellaterra 08193, Spain.
[Raue, Martin] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Wagner, Stefan] Landessternwarte Heidelberg, D-69117 Heidelberg, Germany.
RP Colin, P (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
EM colin@mppmu.mpg.de
OI Mazin, Daniel/0000-0002-2010-4005
NR 19
TC 0
Z9 0
U1 0
U2 1
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0218-2718
J9 INT J MOD PHYS D
JI Int. J. Mod. Phys. D
PD OCT
PY 2009
VL 18
IS 10
BP 1493
EP 1498
DI 10.1142/S0218271809015400
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 512CK
UT WOS:000271220300004
ER
PT J
AU Bellwood, DR
Meyer, CP
AF Bellwood, David R.
Meyer, Christopher P.
TI Endemism and evolution in the Coral Triangle: a call for clarity
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Letter
DE Biodiversity; centre of accumulation; centre of origin; conservation
biogeography; coral reef; hotspots; Indo-Australian Archipelago;
molecular phylogeny
ID BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY; INDO-PACIFIC; REEFS;
CONSERVATION; DIVERSITY; ORIGINS
AB In a recent paper (Bellwood & Meyer, Journal of Biogeography, 2009, 36, 569-576), we critically evaluated the utility of marine endemics for marking the geographical origins of species. In reply, Briggs (2009) identified two issues that needed clarification: (1) whether endemics are assumed to mark the geographical origins of species or areas of exceptionally high rates of origination, and (2) whether our evaluation of the role of endemics disproves the centre of origin hypothesis. Of these two issues, the first can be clearly resolved by recourse to the original literature that explicitly states that it has been assumed that endemics do indeed mark the probable sites of origin of species. The second is equally clear: our evidence does not and can not disprove the centre of origin theory. We suggest, however, that the current data, and endemics in particular, provide limited support for centre of origin theories and that they are more consistent with some centre of accumulation theories. The Indo-Australian Archipelago (IAA; Coral Triangle) therefore appears to be an area where species persist, a centre of survival, regardless of the site of origin of species.
C1 [Bellwood, David R.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld, Australia.
[Bellwood, David R.] James Cook Univ, Ctr Excellence Coral Reef Studies, Townsville, Qld, Australia.
[Meyer, Christopher P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Bellwood, DR (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld, Australia.
EM david.bellwood@jcu.edu.au
NR 17
TC 11
Z9 11
U1 2
U2 19
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD OCT
PY 2009
VL 36
IS 10
BP 2011
EP 2012
DI 10.1111/j.1365-2699.2009.02167.x
PG 2
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 497PA
UT WOS:000270070900019
ER
PT J
AU Puebla, O
AF Puebla, O.
TI Ecological speciation in marine v. freshwater fishes
SO JOURNAL OF FISH BIOLOGY
LA English
DT Review
DE adaptive radiation; ecology; molecular genetics; natural selection;
reproductive isolation; sexual selection
ID CORAL-REEF FISHES; AFRICAN CICHLID FISHES; GREAT-BARRIER-REEF; TUNING
SPECTRAL SENSITIVITY; CODON-SUBSTITUTION MODELS; ANCIENT SPECIES FLOCKS;
OPSIN GENE-EXPRESSION; LAKE MALAWI CICHLIDS; PAIRS COREGONUS SP.;
SYMPATRIC SPECIATION
AB Absolute barriers to dispersal are not common in marine systems, and the prevalence of planktonic larvae in marine taxa provides potential for gene flow across large geographic distances. These observations raise the fundamental question in marine evolutionary biology as to whether geographic and oceanographic barriers alone can account for the high levels of species diversity observed in marine environments such as coral reefs, or whether marine speciation also operates in the presence of gene flow between diverging populations. In this respect, the ecological hypothesis of speciation, in which reproductive isolation results from divergent or disruptive natural selection, is of particular interest because it may operate in the presence of gene flow. Although important insights into the process of ecological speciation in aquatic environments have been provided by the study of freshwater fishes, comparatively little is known about the possibility of ecological speciation in marine teleosts. In this study, the evidence consistent with different aspects of the ecological hypothesis of speciation is evaluated in marine fishes. Molecular approaches have played a critical role in the development of speciation hypotheses in marine fishes, with a role of ecology suggested by the occurrence of sister clades separated by ecological factors, rapid cladogenesis or the persistence of genetically and ecologically differentiated species in the presence of gene flow. Yet, ecological speciation research in marine fishes is still largely at an exploratory stage. Cases where the major ingredients of ecological speciation, namely a source of natural divergent or disruptive selection, a mechanism of reproductive isolation and a link between the two have been explicitly documented are few. Even in these cases, specific predictions of the ecological hypothesis of speciation remain largely untested. Recent developments in the study of freshwater fishes illustrate the potential for molecular approaches to address specific questions related to the ecological hypothesis of speciation such as the nature of the genes underlying key ecological traits, the magnitude of their effect on phenotype and the mechanisms underlying their differential expression in different ecological contexts. The potential provided by molecular studies is fully realized when they are complemented with alternative (e.g. ecological, theoretical) approaches.
C1 [Puebla, O.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Puebla, O (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield Ave, Montreal, PQ H3A 1B1, Canada.
EM oscar.puebla@mail.mcgill.ca
FU Levinson Family; Astroff- Buckshon Family; McGill University;
Smithsonian Tropical Research Institute
FX I acknowledge the financial support from the Levinson Family, the
Astroff- Buckshon Family, McGill University and the Smithsonian Tropical
Research Institute. Thanks to P. Humann, M. A. McCartney, D. Schluter,
J. T. Streelman, N. Tripathi, M. W. Westneat as well as Blackwell
Publishing, Elsevier, Oxford University Press, New World Publications
and the Royal Society for permission to use published photographs and
figures.
NR 236
TC 31
Z9 32
U1 9
U2 76
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-1112
J9 J FISH BIOL
JI J. Fish Biol.
PD OCT
PY 2009
VL 75
IS 5
BP 960
EP 996
DI 10.1111/j.1095-8649.2009.02358.x
PG 37
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 515TS
UT WOS:000271496400002
PM 20738594
ER
PT J
AU Vergara-Chen, C
Gonzalez-Wanguemert, M
Bermingham, E
D'Croz, L
AF Vergara-Chen, C.
Gonzalez-Wanguemert, M.
Bermingham, E.
D'Croz, L.
TI Identification of weakfish Cynoscion (Gill) in the Bay of Panama with
RFLP markers
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE cytochrome b; fish larvae; marine fish; mitochondrial DNA; PCR-RFLP;
species identification
ID MACRODON-ANCYLODON SCIAENIDAE; ATLANTIC COASTAL WATERS; SOUTH-AMERICA;
PERCIFORMES
AB A molecular approach, polymerase chain reaction-restriction fragment length polymorphism (PCR-RFLP), was developed to identify the planktonic larvae of Cynoscion species. Species-specific mitochondrial DNA markers were developed using three restriction endonucleases (DdeI, HaeIII and HinfI). These markers permitted the accurate discrimination of the five Cynoscion species in the Bay of Panama.
C1 [Vergara-Chen, C.; Gonzalez-Wanguemert, M.] Univ Murcia, Fac Biol, Dept Ecol & Hidrol, E-30100 Murcia, Spain.
[D'Croz, L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Bermingham, E.; D'Croz, L.] Estafeta Univ, Univ Panama, Dept Biol Marina & Limnol, Panama City, Panama.
RP Vergara-Chen, C (reprint author), Univ Murcia, Fac Biol, Dept Ecol & Hidrol, Campus Espinardo, E-30100 Murcia, Spain.
EM carlos.vergara@alu.um.es
RI Gonzalez-Wanguemert, Mercedes/M-3467-2013;
OI Gonzalez-Wanguemert, Mercedes/0000-0002-0656-358X; Vergara-Chen,
Carlos/0000-0002-6314-3231
FU Corporacion Elektra Noreste; STRI
FX The Smithsonian Tropical Research Institute (STRI) provided financial
support to carried out this research and C. V.-C. was supported by a
marine science research grant from the Corporacion Elektra Noreste and
STRI. We would like to thank two anonymous referees for their valuable
contributions.
NR 19
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-1112
J9 J FISH BIOL
JI J. Fish Biol.
PD OCT
PY 2009
VL 75
IS 5
BP 1101
EP 1107
DI 10.1111/j.1095-8649.2009.02356.x
PG 7
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 515TS
UT WOS:000271496400009
PM 20738601
ER
PT J
AU Georgescu, MD
Huber, BT
AF Georgescu, Marius D.
Huber, Brian T.
TI EARLY EVOLUTION OF THE CRETACEOUS SERIAL PLANKTIC FORAMINIFERA (LATE
ALBIAN-CENOMANIAN)
SO JOURNAL OF FORAMINIFERAL RESEARCH
LA English
DT Article
ID JERSEY COASTAL-PLAIN; PIENINY-KLIPPEN BELT; TAXONOMIC REVISION;
NORTH-ATLANTIC; BIOSTRATIGRAPHY; RECOGNITION; GENUS
AB The classification of the late Albian-Cenomanian biserial planktic foraminiferal family Heterohelicidae Cushman, 1927, is reevaluated. This group underwent a period of relatively slow evolutionary change during the late Albian-early Cenomanian followed by rapid evolution in the middle Cenomanian. Three new heterohelicid genera and species in the late Albian-early Turonian are described: Protoheterohelix obscura, Planoheterohelix postmoremani, and Glohoheterohelix paraglobulosa. Two reassigned species are also emended: Protoheterohelix washitensis (Tappan) and Planoheterohelix moremani (Cushman). Reassessment of the taxonomic significance of morphological features of the heterohelicid test leads to the conclusion that the most important characters in their taxonomy are test architecture, symmetry/asymmetry of the periapertural structures, nature of periapertural structures, relative size difference of the proloculus and second chamber, test ornamentation, and pore size. Most heterohelicid taxa of the late Albian-Cenomanian display microperforate test walls. Heterohelix Ehrenberg, 1843, which evolved in the early Turonian, is a distinct lineage.
C1 [Georgescu, Marius D.] Univ Calgary, Calgary, AB T2N 1N4, Canada.
[Huber, Brian T.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Georgescu, MD (reprint author), Univ Calgary, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM dgeorge@ucalgary.ca
FU National Museum of Natural History, Smithsonian Institution, Washington,
D.C
FX The data for this article were collected during a postdoctoral
fellowship of the senior author at the National Museum of Natural
History, Smithsonian Institution, Washington, D.C. The unlimited access
to collections (Cushman Collection, Loeblich and Tappan Topotype
Collection, Van Morkhoven Collection, DSDP/ODP Micropaleontological
Reference Center Collection), documentation resources and research
facilities are gratefully acknowledged. Drs R. Mark Leckie (University
of Massachusetts, Amherst) and Isabella Premoli Silva (University of
Milan, Italy) are thanked for reviewing the manuscript. Drs Kenneth L.
Finger (Editor) and Maria Rose Petrizzo (Associate Editor) are thanked
for the guidance during the editorial process. The authors thank IODP
for allowing the resampling of the Blake Plateau ODP Holes 1049B, 1050C
and 1052E, equatorial Central Pacific DSDP Site 463 and Yucatan outer
shelf DSDP Site 95, which proved of paramount importance in developing
this study. Mr. S. Whittaker (NMNH, Smithsonian Institution) is thanked
for his enthusiastic and professional help during the scanning electron
microscope operations.
NR 85
TC 8
Z9 10
U1 0
U2 2
PU CUSHMAN FOUNDATION FORAMINIFERAL RES
PI CAMBRIDGE
PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST,
HARVARD UNIV, CAMBRIDGE, MA 02138 USA
SN 0096-1191
J9 J FORAMIN RES
JI J. Foraminifer. Res.
PD OCT
PY 2009
VL 39
IS 4
BP 335
EP 360
PG 26
WC Paleontology
SC Paleontology
GA 514ZN
UT WOS:000271435800007
ER
PT J
AU Langley, HD
AF Langley, Harold D.
TI Manila and Santiago: The New Steel Navy in the Spanish-American War.
SO JOURNAL OF MILITARY HISTORY
LA English
DT Book Review
C1 [Langley, Harold D.] Smithsonian Inst, Washington, DC 20560 USA.
RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SOC MILITARY HISTORY
PI LEXINGTON
PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA
24450-1600 USA
SN 0899-3718
J9 J MILITARY HIST
JI J. Mil. Hist.
PD OCT
PY 2009
VL 73
IS 4
BP 1351
EP 1352
PG 2
WC History
SC History
GA 503TP
UT WOS:000270563400049
ER
PT J
AU Maderson, PFA
Hillenius, WJ
Hiller, U
Dove, CC
AF Maderson, Paul F. A.
Hillenius, Willem J.
Hiller, Uwe
Dove, Carla C.
TI Towards a Comprehensive Model of Feather Regeneration
SO JOURNAL OF MORPHOLOGY
LA English
DT Article
DE epidermis; feather regeneration; feather SEM; beta-keratin;
alpha-keratin; spathe; calamus; superior umbilicus
ID EVOLUTIONARY ORIGIN; BARB RIDGES; BILATERAL GYNANDROMORPHISM; AVIAN
EPIDERMIS; KERATINIZATION; DIVERSIFICATION; LOCALIZATION; CHICK; CELLS;
CORNIFICATION
AB Understanding of the regeneration of feathers, despite a 140 year tradition of study, has remained substantially incomplete. Moreover, accumulated errors and mis-statements in the literature have confounded the intrinsic difficulties in describing feather regeneration. Lack of allusion to Rudall's (Rudall [1947] Biochem Biophys Acta. 1:549-562) seminal X-ray diffraction study that revealed two distinct keratins, beta- and alpha-, in a mature feather, is one of the several examples where lack of citation long inhibited progress in understanding. This article reviews and reevaluates the available literature and provides a synthetic, comprehensive, morphological model for the regeneration of a generalized, adult contour feather. Particular attention is paid to several features that have previously been largely ignored. Some of these, such as the beta-keratogenic sheath and the alpha-keratogenic, supra-umbilical, pulp caps, are missing from mature, functional feathers sensu stricto because they are lost through preening, but these structures nevertheless play a critical role in development. A new developmental role for a tissue unique to feathers, the medullary pith of the rachis and barb rami, and especially its importance in the genesis of the superior umbilical region (SUR) that forms the transition from the spathe (rachis and vanes) to the calamus, is described. It is postulated that feathers form through an intricate interplay between cyto- and histodifferentiative processes, determined by patterning signals that emanate from the dermal core, and a suite of interacting bio-mechanical forces. Precisely regulated patterns of loss of intercellular adhesivity appear to be the most fundamental aspect of feather morphogenesis and regeneration: rather than a hierarchically branched structure, it appears more appropriate to conceive of feathers as a sheet of mature keratinocytes that is "full of holes. J. Morphol. 270:1166-1208, 2009. (C) 2009 Wiley-Liss, Inc.
C1 [Maderson, Paul F. A.] CUNY Brooklyn Coll, Dept Biol, Brooklyn, NY 11210 USA.
[Hillenius, Willem J.] Coll Charleston, Dept Biol, Charleston, SC 29424 USA.
[Hiller, Uwe] Univ Munster, Inst Anat, D-48149 Munster, Germany.
[Dove, Carla C.] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Maderson, PFA (reprint author), 210 Axehandle Rd, Quakertown, PA 18951 USA.
EM paulmaderson@verizon.net
NR 94
TC 12
Z9 13
U1 0
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0362-2525
EI 1097-4687
J9 J MORPHOL
JI J. Morphol.
PD OCT
PY 2009
VL 270
IS 10
BP 1166
EP 1208
DI 10.1002/jmor.10747
PG 43
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 501ZO
UT WOS:000270423600002
PM 19396862
ER
PT J
AU Bohm, SM
Kalko, EKV
AF Boehm, Stefan M.
Kalko, Elisabeth K. V.
TI Patterns of resource use in an assemblage of birds in the canopy of a
temperate alluvial forest
SO JOURNAL OF ORNITHOLOGY
LA English
DT Article
DE Foraging technique; Acer; Quercus; Niche partitioning; Stratification
ID WOODPECKER DENDROCOPOS-MEDIUS; FORAGING INSECTIVOROUS BIRDS; NORTHERN
HARDWOODS FOREST; TREE-SPECIES PREFERENCES; BEHAVIOR; TITS; SWITZERLAND;
ABUNDANCE; MIGRANTS; TACTICS
AB In our study, we assessed patterns of resource use in an assemblage of birds by observing their foraging behaviour from a crane in the canopy of a temperate alluvial forest. We selected 12 bird species and addressed seasonal changes in feeding activity during a 2-month period in spring focussing on average staying time and utilisation of crown strata in two tree species, the common oak (Quercus robur) and the sycamore maple (Acer pseudoplatanus). We further examined ecological characteristics of the trees (i.e., crown density) that are likely to influence resource use in birds. The selected birds differed in their preference for the tree species. Most birds preferred common oaks. This preference was probably associated with higher food abundance related to substrate characteristics (i.e., roughness of bark) which offer more micro-habitats for arthropods and thus permit higher densities of potential prey. Some bird species switched feeding preferences within the study period from sycamore maples to common oaks in association with tree phenology. We found two main foraging techniques. All birds searched for prey at short distance (<= 50 cm) and gleaned food from substrate except the Pied Flycatcher that foraged by hovering and searched over longer distances (> 50 cm). Overall, we demonstrate in our study that canopy access with mobile crane systems provides excellent opportunities to observe canopy birds and enables detailed analysis of their foraging behaviour. The main result of our study reveals fine-grained resource partitioning of birds within the canopy as an important factor structuring assemblages, with species-specific and in part also seasonal differences in stratification and substrate use.
C1 [Boehm, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Bohm, SM (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
EM stefan.boehm@uni-ulm.de; Elisabeth.Kalko@uni-ulm.de
FU Martin Unterseher; Franz Bairlein; Ophir Tal; Martin Pfeiffer; Marco
Tschapka
FX We dedicate this study to Wilfried Morawetz, founder of the LAK-project,
former professor and head of the Botanical Institute (Biology 1) of the
University of Leipzig, who, with his visionary ideas how to access the
canopy as one of the last frontiers in ecological research, has created
a unique research platform. Furthermore, we are grateful to all
colleagues who helped during the study period and the data analysis. In
particular, we thank Martin Unterseher, Franz Bairlein, Ophir Tal,
Martin Pfeiffer and Marco Tschapka for support. Our study complies with
the current laws of Germany.
NR 49
TC 12
Z9 12
U1 3
U2 24
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0021-8375
J9 J ORNITHOL
JI J. Ornithol.
PD OCT
PY 2009
VL 150
IS 4
BP 799
EP 814
DI 10.1007/s10336-009-0401-7
PG 16
WC Ornithology
SC Zoology
GA 500FI
UT WOS:000270283700009
ER
PT J
AU Turner, BL
Weckstrom, K
AF Turner, Benjamin L.
Weckstrom, Kaarina
TI Phytate as a novel phosphorus-specific paleo-indicator in aquatic
sediments
SO JOURNAL OF PALEOLIMNOLOGY
LA English
DT Article
DE Inositol phosphate; Paleo-indicator; Phosphorus; Phytate; Sediment;
Solution (31)P NMR spectroscopy
ID NUCLEAR-MAGNETIC-RESONANCE; P-31 NMR-SPECTROSCOPY; SOIL ORGANIC
PHOSPHORUS; INOSITOL HEXAPHOSPHATE; LAKE-SEDIMENTS; BALTIC SEA;
INORGANIC PHOSPHORUS; SUBFOSSIL DIATOMS; BAY; EUTROPHICATION
AB A reliable geochemical paleo-indicator for phosphorus remains elusive, despite the importance of understanding historical changes in the nutrient status of aquatic ecosystems. We assessed the potential of phytate (salts of myo-inositol hexakisphosphate) as a novel phosphorus-specific paleo-indicator by measuring its concentrations in dated sediments from an embayment in Helsinki, Finland, with a known 200-year history of trophic changes. Phytate was extracted in a solution containing sodium hydroxide and EDTA and detected by solution (31)P NMR spectroscopy with spectral deconvolution. Concentrations varied markedly with sediment depth and paralleled previously determined changes in diatom assemblages and geochemical indicators linked to trophic status. In contrast, total sediment phosphorus did not reflect phosphorus inputs to the embayment, presumably due to the mobilization of inorganic phosphate under anoxic conditions during periods of high pollutant loading. Importantly, phytate appeared to be stable in these brackish sediments, in contrast to other organic and inorganic phosphates which declined abruptly with depth. We therefore conclude that phytate represents a potentially important indicator of historical changes in phosphorus inputs to water bodies, although additional studies are required to confirm its stability under conditions likely to be encountered in lakes and coastal ecosystems.
C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Weckstrom, Kaarina] Geol Survey Denmark & Greenland, Dept Quaternary Geol, DK-1350 Copenhagen, Denmark.
[Weckstrom, Kaarina] Austrian Acad Sci, Inst Limnol, A-5310 Mondsee, Austria.
RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM TurnerBL@si.edu
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
NR 49
TC 25
Z9 25
U1 0
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0921-2728
J9 J PALEOLIMNOL
JI J. Paleolimn.
PD OCT
PY 2009
VL 42
IS 3
BP 391
EP 400
DI 10.1007/s10933-008-9283-6
PG 10
WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology
SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology
GA 495TQ
UT WOS:000269918300007
ER
PT J
AU Handy, SM
Bachvaroff, TR
Timme, RE
Coats, DW
Kim, S
Delwiche, CF
AF Handy, Sara M.
Bachvaroff, Tsvetan R.
Timme, Ruth E.
Coats, D. Wayne
Kim, Sunju
Delwiche, Charles F.
TI PHYLOGENY OF FOUR DINOPHYSIACEAN GENERA (DINOPHYCEAE, DINOPHYSIALES)
BASED ON rDNA SEQUENCES FROM SINGLE CELLS AND ENVIRONMENTAL SAMPLES
SO JOURNAL OF PHYCOLOGY
LA English
DT Article
DE dinoflagellate; Dinophysiaceae; Dinophysis; environmental clones;
Histioneis; Ornithocercus; Phalacroma; phylogeny
ID REAL-TIME PCR; DINOFLAGELLATE GENUS; MEXICAN PACIFIC; TREE SELECTION;
DNA-SEQUENCES; WATERS; ORNITHOCERCUS; VARIABILITY; ALIGNMENT; DYNAMICS
AB Dinoflagellates are a highly diverse and environmentally important group of protists with relatively poor resolution of phylogenetic relationships, particularly among heterotrophic species. We examined the phylogeny of several dinophysiacean dinoflagellates using samples collected from four Atlantic sites. As a rule, 3.5 kb of sequence including the nuclear ribosomal genes SSU, 5.8S, LSU, plus their internal transcribed spacer (ITS) 1 and 2 regions were determined for 26 individuals, including representatives of two genera for which molecular data were previously unavailable, Ornithocercus F. Stein and Histioneis F. Stein. In addition, a clone library targeting the dinophysiacean ITS2 and LSU sequences was constructed from bulk environmental DNA from three sites. Three phylogenetic trees were inferred from the data, one using data from this study for cells identified to genus or species (3.5 kb, 28 taxa); another containing dinoflagellate SSU submissions from GenBank and the 12 new dinophysiacean sequences (1.9 kb, 56 taxa) from this study; and the third tree combing data from identified taxa, dinophysiacean GenBank submissions, and the clone libraries from this study (2.1 kb, 136 taxa). All trees were congruent and indicated a distinct division between the genera Phalacroma F. Stein and Dinophysis Ehrenb. The cyanobionts containing genera Histioneis and Ornithocercus were also monophyletic. This was the largest molecular phylogeny of dinophysoid taxa performed to date and was consistent with the view that the genus Phalacroma may not be synonymous with Dinophysis.
C1 [Handy, Sara M.; Timme, Ruth E.; Delwiche, Charles F.] Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA.
[Delwiche, Charles F.] Univ Maryland, Maryland Agr Expt Stn, College Pk, MD 20742 USA.
[Bachvaroff, Tsvetan R.; Coats, D. Wayne; Kim, Sunju] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Delwiche, CF (reprint author), Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA.
EM delwiche@umd.edu
RI Handy, Sara/C-6195-2008; Timme, Ruth/C-6543-2008;
OI Delwiche, Charles/0000-0001-7854-8584
FU National Science Foundation [EF-0629624]
FX National Science Foundation funded this work through an Assembling the
Tree of Life grant to C. D., D. W. C. and collaborators(#EF-0629624). We
thank the crew of the R/V Sharpe for their assistance with sampling,
along with P. I. Dr. Robert Mason for providing us with ship time and
research space, Ismael Garate Lizarraga for help with locating important
literature, and Gregg Mendez for help with sample collection. We also
are thankful to Dr. Holly Bowers for use of alignment data, Dr. John
Hall for help with taxonomic questions, two anonymous reviewers for
greatly improving the manuscript, and Garrett Miller for dinoflagellate
illustrations. This manuscript represents contribution number 778 of the
Smithsonian Marine Station, Fort Pierce, FL.
NR 62
TC 20
Z9 20
U1 4
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-3646
EI 1529-8817
J9 J PHYCOL
JI J. Phycol.
PD OCT
PY 2009
VL 45
IS 5
BP 1163
EP 1174
DI 10.1111/j.1529-8817.2009.00738.x
PG 12
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 508BM
UT WOS:000270901800019
PM 27032361
ER
PT J
AU Liu, Y
Wang, R
Paul, VJ
Luesch, H
AF Liu, Y.
Wang, R.
Paul, V. J.
Luesch, H.
TI Novel natural activators of the antioxidant response element
SO JOURNAL OF THE NEUROLOGICAL SCIENCES
LA English
DT Meeting Abstract
CT 19th World Congress of Neurology
CY OCT 24-30, 2009
CL Bangkok, THAILAND
C1 [Liu, Y.; Wang, R.; Luesch, H.] Univ Florida, Gainesville, FL USA.
[Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-510X
J9 J NEUROL SCI
JI J. Neurol. Sci.
PD OCT
PY 2009
VL 285
SU 1
BP S169
EP S169
PG 1
WC Clinical Neurology; Neurosciences
SC Neurosciences & Neurology
GA 529ML
UT WOS:000272521300583
ER
PT J
AU Nunes, F
Norris, RD
Knowlton, N
AF Nunes, F.
Norris, R. D.
Knowlton, N.
TI Implications of isolation and low genetic diversity in peripheral
populations of an amphi-Atlantic coral
SO MOLECULAR ECOLOGY
LA English
DT Article
DE connectivity; coral; genetic diversity; Montastraea cavernosa;
peripheral population
ID MICROSATELLITE LOCI; CARIBBEAN CORAL; REEF FISH; POCILLOPORA-DAMICORNIS;
MONTASTRAEA-ANNULARIS; LARVAL BEHAVIOR; LITOPENAEUS-SCHMITTI; GENOTYPIC
DIVERSITY; SEXUAL REPRODUCTION; MARINE POPULATIONS
AB Limited dispersal and connectivity in marine organisms can have negative fitness effects in populations that are small and isolated, but reduced genetic exchange may also promote the potential for local adaptation. Here, we compare the levels of genetic diversity and connectivity in the coral Montastraea cavernosa among both central and peripheral populations throughout its range in the Atlantic. Genetic data from one mitochondrial and two nuclear loci in 191 individuals show that M. cavernosa is subdivided into three genetically distinct regions in the Atlantic: Caribbean-North Atlantic, Western South Atlantic (Brazil) and Eastern Tropical Atlantic (West Africa). Within each region, populations have similar allele frequencies and levels of genetic diversity; indeed, no significant differentiation was found between populations separated by as much as 3000 km, suggesting that this coral species has the ability to disperse over large distances. Gene flow within regions does not, however, translate into connectivity across the entire Atlantic. Instead, substantial differences in allele frequencies across regions suggest that genetic exchange is infrequent between the Caribbean, Brazil and West Africa. Furthermore, markedly lower levels of genetic diversity are observed in the Brazilian and West African populations. Genetic diversity and connectivity may contribute to the resilience of a coral population to disturbance. Isolated peripheral populations may be more vulnerable to human impacts, disease or climate change relative to those in the genetically diverse Caribbean-North Atlantic region.
C1 [Nunes, F.; Norris, R. D.; Knowlton, N.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Knowlton, N.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20012 USA.
RP Nunes, F (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, 9500 Gilman Dr,MC 0208, La Jolla, CA 92093 USA.
EM fnunes@ucsd.edu
RI Nunes, Flavia/B-5041-2011
OI Nunes, Flavia/0000-0002-3947-6634
FU John Dove Isaacs Chair in Natural Philosophy to NK
FX We thank A. Sole-Cava for the use of his laboratory facilities at the
Federal University of Rio de Janeiro for molecular work on Brazilian
corals, J.M. Pandolfi and E. F. Weil for providing samples for this
study and N. Le Dantec, K.J. Nichols, B. M. Feitoza and J.E.P. Freitas
for assistance in sample collection. Comments from R. S. Burton, S. V.
Vollmer, S. R. Palumbi and four anonymous reviewers improved this
manuscript. This work was supported by the John Dove Isaacs Chair in
Natural Philosophy to NK and by an anonymous private donation to the SIO
Graduate Department to FN.
NR 85
TC 30
Z9 31
U1 2
U2 22
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0962-1083
J9 MOL ECOL
JI Mol. Ecol.
PD OCT
PY 2009
VL 18
IS 20
BP 4283
EP 4297
DI 10.1111/j.1365-294X.2009.04347.x
PG 15
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 505CM
UT WOS:000270665900014
PM 19765228
ER
PT J
AU Pearson, C
Khan, SA
AF Pearson, Chris
Khan, Sophia A.
TI Submillimetre surveys: the prospects for Herschel
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; Galaxy: evolution
ID UNIVERSE GALAXY SURVEY; STAR-FORMATION; NUMBER COUNTS; HIGH-REDSHIFT;
LOCKMAN HOLE; CONFUSION; SPITZER; PREDICTIONS; LUMINOSITY; EVOLUTION
AB Using the observed submillimetre source counts, from 250 to 1200 mu m [including the most recent 250, 350 and 500 mu m counts from Balloon-borne Large-Aperture Submillimetre Telescope (BLAST)], we present a model capable of reproducing these results, which is used as a basis to make predictions for upcoming surveys with the Spectral and Photometric Imaging Receive (SPIRE) instrument aboard the Herschel Space Observatory. The model successfully fits both the integral and differential source counts of submillimetre galaxies in all wavebands, predicting that while ultra-luminous infrared (IR) galaxies dominate at the brightest flux densities, the bulk of the IR background is due to the less luminous IR galaxy population. The model also predicts confusion limits and contributions to the cosmic IR background that are consistent with the BLAST results. Applying this to SPIRE gives predicted source confusion limits of 19.4, 20.5 and 16.1 mJy in the 250, 350 and 500 mu m bands, respectively. This means the SPIRE surveys should achieve sensitivities 1.5 times deeper than the BLAST, revealing a fainter population of IR-luminous galaxies and detecting approximately 2600, 1300 and 700 sources per deg(2) in the SPIRE bands (with one in three sources expected to be a high-redshift ultra-luminous source at 500 mu m). The model number redshift distributions predict a bimodal distribution of local quiescent galaxies and a high-redshift peak corresponding to strongly evolving star-forming galaxies. It suggests the very deepest surveys with Herschel-SPIRE ought to sample the source population responsible for the bulk of the IR background.
C1 [Pearson, Chris] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Pearson, Chris] Univ Lethbridge, Dept Phys, Lethbridge, AB T1J 1B1, Canada.
[Pearson, Chris] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Khan, Sophia A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Khan, Sophia A.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China.
RP Pearson, C (reprint author), Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
EM chris.pearson@stfc.ac.uk
NR 45
TC 17
Z9 17
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2009
VL 399
IS 1
BP L11
EP L15
DI 10.1111/j.1745-3933.2009.00706.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 678WM
UT WOS:000284113800003
ER
PT J
AU Colombo, LPL
Pierpaoli, E
Pritchard, JR
AF Colombo, L. P. L.
Pierpaoli, E.
Pritchard, J. R.
TI Cosmological parameters after WMAP5: forecasts for Planck and future
galaxy surveys
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: statistics; cosmic microwave background; cosmological
parameters; large-scale structure of Universe
ID MICROWAVE BACKGROUND DATA; DARK ENERGY; REDSHIFT SURVEYS; POWER SPECTRA;
SCALAR FIELD; ANISOTROPY; MATTER; POLARIZATION; REIONIZATION;
CONSTRAINTS
AB With its increased sensitivity and resolution, the Planck satellite is expected to improve the measurement of most cosmological parameters by several factors with respect to current Wilkinson Microwave Anisotropy Probe results. The actual performance, however, may depend upon various aspects of the data analysis. In this paper, we analyse the impact of specifics of the data analysis on the actual final results. We also explore the synergies in combining Planck results with future galaxy surveys. We find that Planck will improve constraints on most cosmological parameters by a factor of 3-4 and on the tensor-to-scalar ratio r by a factor of 9. Also, inflationary parameters, like r, n(s) and n(run), are practically not degenerate any longer. The tensor spectral index, however, is little constrained. A combination of the 70 to 143 GHz channels will contain about 90 per cent of all possible information, with 143 GHz polarization information carrying about half of the constraining power on r. Also, the error on r degrades by a factor of 2 if no B modes are considered in the analysis. High-l temperature information is essential for determination of n(s) and (b), while improving noise properties increases the l-range where Planck would be cosmic-variance-limited in polarization, implying a significant improvement on the determination of r, tau and A(s). However, a sub-per-cent difference in the full width at half-maximum used in the data analysis with respect to the one in the map will result in a bias for several parameters. Finally, Planck will greatly help future missions like Large Synoptic Survey Telescope and Cosmic Inflation Probe reach their potentials by providing tight constraints on parameters like n(s) and n(run). Considering Planck together with these probes will help in breaking degeneracies between (K) and (Lambda) or (dm) and f(nu), resulting in improvements of several factors in the error associated with these parameters.
C1 [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Los Angeles, CA 90089 USA.
[Pritchard, J. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Colombo, LPL (reprint author), Univ So Calif, Los Angeles, CA 90089 USA.
EM colombo@usc.edu
RI Colombo, Loris/J-2415-2016;
OI Colombo, Loris/0000-0003-4572-7732; Pritchard,
Jonathan/0000-0003-4127-5353; Pierpaoli, Elena/0000-0002-7957-8993
FU NSF-ADVANCE [AST-0649899]; JPL SURP [1314616]; NASA [NNX07AH59G,
HST-HF-01211.01-A]; Space Telescope Science Institute; Universities for
Research in Astronomy, Inc., for NASA [NAS 5-26555]; [1290790]
FX EP is an NSF-ADVANCE fellow (AST-0649899) also supported by JPL SURP
award 1314616. LPLC and EP were supported by NASA grant NNX07AH59G and
Planck subcontract 1290790 for this work, and would like to thank
Caltech for hospitality during this period. JRP is supported by NASA
through Hubble Fellowship grant HST-HF-01211.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. We acknowledge the use of the cosmomc, pico and healpix
packages. The authors thank Kevin Huffenberger and Brendan Crill for
stimulating discussion on beams effect.
NR 66
TC 33
Z9 33
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 OCT 1
PY 2009
VL 398
IS 4
BP 1621
EP 1637
DI 10.1111/j.1365-2966.2009.14802.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495PQ
UT WOS:000269906400003
ER
PT J
AU Mannucci, F
Cresci, G
Maiolino, R
Marconi, A
Pastorini, G
Pozzetti, L
Gnerucci, A
Risaliti, G
Schneider, R
Lehnert, M
Salvati, M
AF Mannucci, F.
Cresci, G.
Maiolino, R.
Marconi, A.
Pastorini, G.
Pozzetti, L.
Gnerucci, A.
Risaliti, G.
Schneider, R.
Lehnert, M.
Salvati, M.
TI LSD: Lyman-break galaxies Stellar populations and Dynamics - I. Mass,
metallicity and gas at z similar to 3.1 star
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: abundances; galaxies: formation; galaxies: high-redshift;
galaxies: starburst
ID STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; INTEGRAL FIELD SPECTROSCOPY;
SPITZER-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; VLT DEEP SURVEY;
CHEMICAL EVOLUTION; FORMATION HISTORY; PHYSICAL-PROPERTIES; STARBURST
GALAXIES
AB We present the first results of a project, Lyman-break galaxies Stellar populations and Dynamics (LSD), aimed at obtaining spatially resolved, near-infrared (IR) spectroscopy of a complete sample of Lyman-break galaxies at z similar to 3. Deep observations with adaptive optics resulted in the detection of the main optical lines, such as [O ii] lambda 3727, H beta and [O iii] lambda 5007, which are used to study sizes, star formation rates (SFRs), morphologies, gas-phase metallicities, gas fractions and effective yields. Optical, near-IR and Spitzer/Infrared Array Camera photometry are used to measure stellar mass. We obtain that morphologies are usually complex, with the presence of several peaks of emissions and companions that are not detected in broad-band images. Typical metallicities are 10-50 per cent solar, with a strong evolution of the mass-metallicity relation from lower redshifts. Stellar masses, gas fraction and evolutionary stages vary significantly among the galaxies, with less massive galaxies showing larger fractions of gas. In contrast with observations in the local universe, effective yields decrease with stellar mass and reach solar values at the low-mass end of the sample. This effect can be reproduced by gas infall with rates of the order of the SFRs. Outflows are present but are not needed to explain the mass-metallicity relation. We conclude that a large fraction of these galaxies is actively creating stars after major episodes of gas infall or merging.
C1 [Mannucci, F.; Cresci, G.; Risaliti, G.; Schneider, R.; Salvati, M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Cresci, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Maiolino, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Marconi, A.; Pastorini, G.; Gnerucci, A.] Univ Florence, Dip Astron & Sci Spazio, I-50125 Florence, Italy.
[Pozzetti, L.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lehnert, M.] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92190 Meudon, France.
RP Mannucci, F (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM filippo@arcetri.astro.it
RI Marconi, Alessandro/C-5880-2009; Schneider, Raffaella/E-4216-2017;
OI Marconi, Alessandro/0000-0002-9889-4238; Schneider,
Raffaella/0000-0001-9317-2888; Pozzetti, Lucia/0000-0001-7085-0412;
Risaliti, Guido/0000-0002-3556-977X; mannucci,
filippo/0000-0002-4803-2381; Cresci, Giovanni/0000-0002-5281-1417
FU Italian Space Agency [ASI-INAF I/016/07/0]; INAF CRAM [1.06.09.10]; NASA
(Spitzer) [1343503]
FX We thank F. Eisenhauer and A. Modigliani for support during data
reduction, and B. Kennicutt and T. Nagao for very useful discussions. We
also thank the staffs of ESO, Spitzer and TNG for excellent service
observing, and E. Daddi for having provided data in tabular form. This
work was partially supported by the Italian Space Agency through
contract ASI-INAF I/016/07/0, by INAF CRAM 1.06.09.10 and by NASA
(Spitzer) grant number 1343503.
NR 113
TC 193
Z9 193
U1 1
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 OCT 1
PY 2009
VL 398
IS 4
BP 1915
EP 1931
DI 10.1111/j.1365-2966.2009.15185.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 495PQ
UT WOS:000269906400026
ER
PT J
AU Jorge, MLSP
Howe, HF
AF Jorge, Maria Luisa S. P.
Howe, Henry F.
TI Can forest fragmentation disrupt a conditional mutualism? A case from
central Amazon
SO OECOLOGIA
LA English
DT Article
DE Brazil; Caviomorph rodents; Seed caching; Seed dispersal; Seasonal
mutualism
ID SEED DISPERSAL; DASYPROCTA-LEPORINA; TROPICAL TREES; RUMPED AGOUTI;
SIZE; ECOLOGY; RODENTS; SURVIVAL; ACOUCHY; PALM
AB This is the first study to investigate whether scatter-hoarding behavior, a conditional mutualism, can be disrupted by forest fragmentation. We examined whether acouchies (Myoprocta acouchy, Rodentia) and agoutis (Dasyprocta leporina, Rodentia) changed scatter-hoarding behavior toward seeds of Astrocaryum aculeatum (Arecaceae) as a consequence of a decrease in forest-patch area. Our study was conducted at the 30-year-old Biological Dynamics of Forest Fragments Project, in central Amazon, Brazil. We tested whether forest size affected the number of Astrocaryum seeds removed and scatter-hoarded (and likely dispersed) by acouchies and agoutis, as well as the distance that the seeds were hoarded. The study extended over three seasons: the peak of the rainy season (March-April), the transition between the rainy and the dry season (May-June), and the peak of the dry season (August-September). Our results revealed that the number of seeds removed was larger in smaller fragments, but that the percentage of seeds hoarded was much lower, and seeds eaten much higher, in 1-ha fragments. Moreover, fewer seeds were taken longer distances in fragments than in the continuous forest. Site affected the number of seeds removed and season affected the percentage of seeds hoarded: more seeds were removed from stations in one site than in two others, and hoarding was more important in April and September than in June. Our study reveals that scatter-hoarding behavior is affected by forest fragmentation, with the most important disruption in very small fragments. Fragmentation converts a largely mutualistic relationship between the rodents and this palm in large forest patches into seed predation in small fragments.
C1 [Jorge, Maria Luisa S. P.] Vanderbilt Univ, Dept Biol Sci, VU Stn, Nashville, TN 37235 USA.
[Jorge, Maria Luisa S. P.; Howe, Henry F.] Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA.
[Jorge, Maria Luisa S. P.; Howe, Henry F.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA.
[Jorge, Maria Luisa S. P.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
[Jorge, Maria Luisa S. P.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil.
RP Jorge, MLSP (reprint author), Vanderbilt Univ, Dept Biol Sci, VU Stn, B 35-1634, Nashville, TN 37235 USA.
EM malu.jorge@vanderbilt.edu; hfhowe@uic.edu
RI Jorge, Maria Luisa/B-1103-2013; Howe, Henry F/B-8749-2014
OI Jorge, Maria Luisa/0000-0003-4264-5897; Howe, Henry
F/0000-0001-5081-2128
FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; BDFFP;
University of Illinois at Chicago; CNPq; NSF [DEB 012908, 0516259]
FX We thank M. L. Dourado, S. M. Souza, A. M. dos Reis and O. F. da Silva,
for invaluable field assistance. Significant comments were provided by
Dr J. Brown, Dr R. Foster, Dr B. Patterson, Dr C. Whelan, Dr P. Banks,
Dr T. Theimer, and one anonymous reviewer. This work was funded by the
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, the BDFFP
and the University of Illinois at Chicago. This is publication no. 531
in the BDFFP technical series. Our experiments comply with the laws in
Brazil. M. L. S. P. J. was supported by CNPq with a Ph. D. scholarship
and H. F. H. was supported by NSF grants DEB 012908 and 0516259 during
the course of this study.
NR 48
TC 18
Z9 20
U1 3
U2 33
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD OCT
PY 2009
VL 161
IS 4
BP 709
EP 718
DI 10.1007/s00442-009-1417-7
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 495AE
UT WOS:000269860700007
PM 19633870
ER
PT J
AU Hu, XS
He, FL
Hubbell, SP
AF Hu, Xin-Sheng
He, Fangliang
Hubbell, Stephen P.
TI Community differentiation on landscapes: drift, migration and speciation
SO OIKOS
LA English
DT Article
ID BETA-DIVERSITY; SPECIES-DIVERSITY; PHYLOGENETIC STRUCTURE; CONCLUDING
REMARKS; SAMPLING FORMULA; GENE FREQUENCIES; NEUTRAL THEORY; POPULATION;
ECOLOGY; CONVERGENCE
AB Theories of the differentiation of ecological communities on landscapes have typically not considered evolutionary dynamics. Here we analytically study the expected differentiation among local communities in a large metacommunity, undergoing speciation, ecological drift and intercommunity dispersal, in the context of neutral theory. We demonstrate that heterogeneity in species diversity and abundance arises among communities when local communities are small and intercommunity migration is infrequent. We propose a new measure to describe community differentiation, defined as the average correlation or the average probability (C(st)) that two randomly sampled individuals of the same species within local communities are from the same ancestor. The effects of driving forces (migration, mutation, and ecological drift) are incorporated into the two-level hierarchical community structure in a finite island model of neutral communities. Community differentiation can increase the effective metacommunity size or the Hubbell's fundamental species diversity in the metacommunity by a factor (1-C(st))-1. Significant community differentiation arises when C(st)not equal 0. Intercommunity migration promotes species diversity in local communities but reduce species diversity in the metacommunity. In either the finite or infinite island case, one can estimate the number of intercommunity migrants by using multiple local community datasets when the speciation is negligible in the neutral local communities, or by using the metacommunity dataset when the speciation is included in the local neutral communities. These results highlight the significance of the evolutionary mechanisms in generating heterogeneous communities in the absence of complicated ecological processes on large landscapes.
C1 [Hu, Xin-Sheng; He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.] APO AA, Unit 0948, Smithsonian Trop Res Inst, Balboa, Panama.
RP Hu, XS (reprint author), Univ Alberta, Dept Renewable Resources, 751 Gen Serv Bldg, Edmonton, AB T6G 2H1, Canada.
EM xin-sheng.hu@ualberta.ca
FU Natural Sciences and Engineering Research Council of Canada; National
Science Foundation
FX We appreciate T. Wiegand and L. Svensson for useful comments and
suggestions that improved the earlier version of this article. The work
was supported by the Natural Sciences and Engineering Research Council
of Canada (FH) and National Science Foundation (SPH).
NR 51
TC 2
Z9 2
U1 1
U2 23
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0030-1299
J9 OIKOS
JI Oikos
PD OCT
PY 2009
VL 118
IS 10
BP 1515
EP 1523
DI 10.1111/j.1600-0706.2009.17233.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 502DO
UT WOS:000270435300009
ER
PT J
AU Erlandson, JM
Rick, TC
Braje, TJ
AF Erlandson, Jon M.
Rick, Torben C.
Braje, Todd J.
TI Fishing up the Food Web?: 12,000 Years of Maritime Subsistence and
Adaptive Adjustments on California's Channel Islands
SO PACIFIC SCIENCE
LA English
DT Article
ID SAN-MIGUEL ISLAND; SOUTHERN-CALIFORNIA; PACIFIC COAST; NORTH-AMERICA;
HUMAN IMPACTS; MARINE; ADAPTATIONS; ARCHAEOLOGY; ECOSYSTEMS; ANTIQUITY
AB Archaeologists working on California's northern Channel Islands have produced an essentially continuous record of Native American fishing and nearshore ecological changes spanning die last 12,000 years. To search for evidence of Pauly's "fishing down the foodweb" pattern typical of recent historical fisheries, we analyzed variation in the dietary importance of major marine faunal classes (shellfish, fish, marine mammals) on the islands through time. Faunal data suggest that the Island Chumash and their predecessors focused primarily on low-trophic-level shellfish during the Early and Middle Holocene, before shifting their economic focus to finfish and pinnipeds during the Late Holocene. Replicated in faunal sequences from the adjacent mainland, this trans-Holocene pattern suggests that Native Americans fished Lip the food web, a strategy that may have been more sustainable and had fewer ecological repercussions. Emerging technological data suggest, however, that some of the earliest Channel Islanders focused more heavily on higher-trophic-level animals, including marine mammals, seabirds, and waterfowl. These data emphasize the differences between the primarily subsistence-based foraging strategies of ancient Channel Islanders and the globalized market-based fisheries of modern and historic times, with important implications for understanding the long-term evolution and historical ecology of marine ecosystems.
C1 [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
[Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA.
[Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA.
[Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA.
RP Erlandson, JM (reprint author), Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
EM jerland@uoregon.edu
OI Erlandson, Jon/0000-0002-4705-4319
FU National Science Foundation; National Park Service; University of
Oregon; Southern Methodist University; National Marine Fisheries
Service; U.S. Navy; Western Parks Association; Foundation for
Exploration and Research on Cultural Origins; Marine Biology
Conservation Institute
FX Research has been supported by grants and other assistance from the
National Science Foundation, National Park Service, University of
Oregon, Southern Methodist University, National Marine Fisheries
Service, U.S. Navy, Western Parks Association, the Foundation for
Exploration and Research on Cultural Origins, and the Marine Biology
Conservation Institute. Manuscript accepted 30 January 2009.
NR 53
TC 32
Z9 33
U1 5
U2 35
PU UNIV HAWAII PRESS
PI HONOLULU
PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA
SN 0030-8870
EI 1534-6188
J9 PAC SCI
JI Pac. Sci.
PD OCT
PY 2009
VL 63
IS 4
SI SI
BP 711
EP 724
DI 10.2984/049.063.0411
PG 14
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 507JN
UT WOS:000270849400011
ER
PT J
AU Tang, LY
Zhang, JY
Yan, ZC
Shi, TY
Babb, JF
Mitroy, J
AF Tang, Li-Yan
Zhang, Jun-Yi
Yan, Zong-Chao
Shi, Ting-Yun
Babb, James F.
Mitroy, J.
TI Calculations of polarizabilities and hyperpolarizabilities for the Be+
ion
SO PHYSICAL REVIEW A
LA English
DT Article
DE atom-ion collisions; beryllium; helium neutral atoms; hydrogen neutral
atoms; lithium; polarisability; positive ions; potential energy
functions; variational techniques; wave functions
ID LITHIUM ISOELECTRONIC SEQUENCE; DIPOLE POLARIZABILITIES;
OSCILLATOR-STRENGTHS; RYDBERG STATES; VARIATIONAL CALCULATIONS;
DISPERSION COEFFICIENTS; MOLECULAR-IONS; GROUND-STATES; COLLISIONS;
SYSTEMS
AB The polarizabilities and hyperpolarizabilities of the Be+ ion in the 2 S-2 state and the 2 P-2 state are determined. Calculations are performed using two independent methods: (i) variationally determined wave functions using Hylleraas basis set expansions and (ii) single electron calculations utilizing a frozen-core Hamiltonian. The first few parameters in the long-range interaction potential between a Be+ ion and a H, He, or Li atom, and the leading parameters of the effective potential for the high-L Rydberg states of beryllium were also computed. All the values reported are the results of calculations close to convergence. Comparisons are made with published results where available.
C1 [Tang, Li-Yan; Shi, Ting-Yun] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China.
[Tang, Li-Yan] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China.
[Zhang, Jun-Yi; Mitroy, J.] Charles Darwin Univ, Sch Engn, Darwin, NT 0909, Australia.
[Yan, Zong-Chao] Chinese Acad Sci, Ctr Cold Atom Phys, Wuhan 430071, Peoples R China.
[Yan, Zong-Chao] Wuhan Univ, Dept Phys, Wuhan 430072, Peoples R China.
[Yan, Zong-Chao] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada.
[Babb, James F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Tang, LY (reprint author), Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China.
RI Shi, Tingyun/I-6022-2013; Mitroy, James/N-2162-2013; Yan,
Zong-Chao/F-6668-2014;
OI Mitroy, James/0000-0002-2477-1251; Babb, James/0000-0002-3883-9501
FU NNSF of China [10674154]; National Basic Research Program of China
[2005CB724508]; NSERC of Canada; ACEnet; SHARCnet; CAS/SAFEA
International Partnership Program
FX This work was supported by NNSF of China under Grant No. 10674154 and by
the National Basic Research Program of China under Grant No.
2005CB724508. Z.-C.Y. was supported by NSERC of Canada and by the
computing facilities of ACEnet, SHARCnet, WestGrid, and in Part by the
CAS/SAFEA International Partnership Program for Creative Research Teams.
J.F.B was supported in part by the U.S. NSF through a grant for the
Institute of Theoretical Atomic, Molecular and Optical Physics at
Harvard University and Smithsonian Astrophysical Observatory. J.M. and
J.Y.Z would like to thank the Wuhan Institute of Physics and Mathematics
for its hospitality during their visits.
NR 52
TC 11
Z9 11
U1 2
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD OCT
PY 2009
VL 80
IS 4
AR 042511
DI 10.1103/PhysRevA.80.042511
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 513VB
UT WOS:000271351000087
ER
PT J
AU Tscherbul, TV
Buchachenko, AA
Dalgarno, A
Lu, MJ
Weinstein, JD
AF Tscherbul, T. V.
Buchachenko, A. A.
Dalgarno, A.
Lu, M. -J.
Weinstein, J. D.
TI Suppression of Zeeman relaxation in cold collisions of P-2(1/2) atoms
SO PHYSICAL REVIEW A
LA English
DT Article
DE ab initio calculations; atom-atom collisions; atomic forces; gallium;
helium neutral atoms; indium; magnetic traps; Zeeman effect
ID POTENTIAL-ENERGY CURVES; OPTICAL LATTICES; ULTRACOLD ATOMS;
DIODE-LASERS; BASIS-SETS; PSEUDOPOTENTIALS; COHERENCE; GALLIUM; GAS; HE
AB We present a combined experimental and theoretical study of angular momentum depolarization in cold collisions of P-2 atoms in the presence of an external magnetic field. We show that collision-induced Zeeman relaxation of Ga(P-2(1/2)) and In(P-2(1/2)) atoms in cold He-4 gas is dramatically suppressed compared to atoms in P-2(3/2) states. Using rigorous quantum-scattering calculations based on ab initio interaction potentials, we demonstrate that Zeeman transitions in collisions of atoms in P-2(1/2) electronic states occur via couplings to the P-2(3/2) state induced by the anisotropy of the interaction potential. Our results suggest the feasibility of sympathetic cooling and magnetic trapping of P-2(1/2)-state atoms, such as halogens, thereby opening up exciting areas of research in precision spectroscopy and cold-controlled chemistry.
C1 [Tscherbul, T. V.; Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
[Tscherbul, T. V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Buchachenko, A. A.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, Russia.
[Lu, M. -J.; Weinstein, J. D.] Univ Nevada, Dept Phys, Reno, NV 89557 USA.
RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
RI Buchachenko, Alexei/C-8452-2012; Tscherbul, Timur/K-3286-2014
OI Buchachenko, Alexei/0000-0003-0701-5531; Tscherbul,
Timur/0000-0001-5689-040X
FU Nevada NASA EPSCoR; joint Russian Basic Research Fund-Consortium
E.I.N.S.T.E.I.N; Chemical Science, Geoscience, and Bioscience Division
of the Office of Basic Energy Science; U.S. Department of Energy; NSF
FX We acknowledge stimulating discussions with John Doyle and Roman Krems.
This work was supported by the Nevada NASA EPSCoR program in
Astrophysics, joint Russian Basic Research Fund-Consortium
E.I.N.S.T.E.I.N project, and the Chemical Science, Geoscience, and
Bioscience Division of the Office of Basic Energy Science, Office of
Science, U. S. Department of Energy and NSF grants to the Harvard-MIT
CUA and ITAMP at Harvard University, and Smithsonian Astrophysical
Observatory.
NR 29
TC 10
Z9 10
U1 1
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD OCT
PY 2009
VL 80
IS 4
AR 040701
DI 10.1103/PhysRevA.80.040701
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 513VB
UT WOS:000271351000009
ER
PT J
AU Xiao, YH
Wang, T
Baryakhtar, M
Camp, M
Crescimanno, M
Hohensee, M
Jiang, L
Phillips, DF
Lukin, MD
Yelin, SF
Walsworth, RL
AF Xiao, Yanhong
Wang, Tun
Baryakhtar, Maria
Van Camp, Mackenzie
Crescimanno, Michael
Hohensee, Michael
Jiang, Liang
Phillips, David F.
Lukin, Mikhail D.
Yelin, Susanne F.
Walsworth, Ronald L.
TI Electromagnetically induced transparency with noisy lasers
SO PHYSICAL REVIEW A
LA English
DT Article
DE laser noise; light coherence; phase noise; quantum optics; self-induced
transparency
ID ATOMIC VAPOR; DIODE-LASER; SPIN NOISE; SPECTROSCOPY; PULSES
AB We demonstrate and characterize two coherent phenomena that can mitigate the effects of laser phase noise for electromagnetically induced transparency (EIT): a laser-power-broadening-resistant resonance in the transmitted intensity cross correlation between EIT optical fields, and a resonant suppression of the conversion of laser phase noise to intensity noise when one-photon noise dominates over two-photon-detuning noise. Our experimental observations are in good agreement with both an intuitive physical picture and numerical calculations. The results have wide-ranging applications to spectroscopy, atomic clocks, and magnetometers.
C1 [Xiao, Yanhong] Fudan Univ, Dept Phys, Surface Phys Lab, Natl Key Lab, Shanghai 200433, Peoples R China.
[Xiao, Yanhong] Fudan Univ, Adv Mat Lab, Shanghai 200433, Peoples R China.
[Xiao, Yanhong; Hohensee, Michael; Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wang, Tun; Yelin, Susanne F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Wang, Tun] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Baryakhtar, Maria; Hohensee, Michael; Jiang, Liang; Lukin, Mikhail D.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Van Camp, Mackenzie] Lawrence Univ, Dept Phys, Appleton, WI 54912 USA.
[Crescimanno, Michael] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA.
[Yelin, Susanne F.] ITAMP, Cambridge, MA 02138 USA.
RP Xiao, YH (reprint author), Fudan Univ, Dept Phys, Surface Phys Lab, Natl Key Lab, Shanghai 200433, Peoples R China.
RI Jiang, Liang/A-9847-2008;
OI Jiang, Liang/0000-0002-0000-9342; Hohensee, Michael/0000-0002-8106-4502
FU ONR; Smithsonian Institution; NSF
FX We are grateful to I. Novikova, J. Kitching, and J. Vanier for useful
discussions. This work was supported by ONR, the Smithsonian
Institution, and NSF.
NR 29
TC 15
Z9 15
U1 1
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD OCT
PY 2009
VL 80
IS 4
AR 041805
DI 10.1103/PhysRevA.80.041805
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 513VB
UT WOS:000271351000026
ER
PT J
AU Schmidt, F
Vikhlinin, A
Hu, W
AF Schmidt, Fabian
Vikhlinin, Alexey
Hu, Wayne
TI Cluster constraints on f(R) gravity
SO PHYSICAL REVIEW D
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; DARK ENERGY; EVOLUTION; CONSTANT; SCATTER
AB Modified gravitational forces in models that seek to explain cosmic acceleration without dark energy typically predict deviations in the abundance of massive dark matter halos. We conduct the first, simulation calibrated, cluster abundance constraints on a modified gravity model, specifically the modified action f(R) model. The local cluster abundance, when combined with geometric and high redshift data from the cosmic microwave background, supernovae, H(0), and baryon acoustic oscillations, improves previous constraints by nearly 4 orders of magnitude in the field amplitude. These limits correspond to a 2 order of magnitude improvement in the bounds on the range of the force modification from the several Gpc scale to the tens of Mpc scale.
C1 [Schmidt, Fabian; Hu, Wayne] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Schmidt, Fabian; Hu, Wayne] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vikhlinin, Alexey] Space Res Inst, Moscow, Russia.
RP Schmidt, F (reprint author), Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
OI Schmidt, Fabian/0000-0002-6807-7464
FU NSF [PHY-0114422, PHY-0551142]; U.S. Department of Energy
[DE-FG02-90ER-40560]; David and Lucile Packard Foundation; NASA
[NAG5-9217, GO5-6120A, GO6-7119X, NAS8-39073]
FX We thank the Aspen Center for Physics where part of this work was
completed. F. S. and W. H. were supported by the Kavli Institute for
Cosmological Physics (KICP) at the University of Chicago through Grants
NSF No. PHY-0114422 and NSF No. PHY-0551142 and an endowment from the
Kavli Foundation and its founder Fred Kavli. W. H. was additionally
supported by the U.S. Department of Energy Contract No.
DE-FG02-90ER-40560 and the David and Lucile Packard Foundation. A. V.
was supported by NASA Grants and Contracts No. NAG5-9217, No. GO5-6120A,
No. GO6-7119X, and No. NAS8-39073. Computational resources for the
cosmological simulations were provided by the KICP-Fermilab computer
cluster.
NR 32
TC 133
Z9 133
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT
PY 2009
VL 80
IS 8
AR 083505
DI 10.1103/PhysRevD.80.083505
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 513WB
UT WOS:000271353700020
ER
PT J
AU Yoo, J
Fitzpatrick, AL
Zaldarriaga, M
AF Yoo, Jaiyul
Fitzpatrick, A. Liam
Zaldarriaga, Matias
TI New perspective on galaxy clustering as a cosmological probe: General
relativistic effects
SO PHYSICAL REVIEW D
LA English
DT Article
ID DIGITAL SKY SURVEY; SPATIAL CORRELATIONS; PERTURBATIONS; ANISOTROPIES;
UNIVERSE
AB We present a general relativistic description of galaxy clustering in a Friedmann-Lemaitre-Robertson-Walker universe. The observed redshift and position of galaxies are affected by the matter fluctuations and the gravity waves between the source galaxies and the observer, and the volume element constructed by using the observables differs from the physical volume occupied by the observed galaxies. Therefore, the observed galaxy fluctuation field contains additional contributions arising from the distortion in observable quantities and these include tensor contributions as well as numerous scalar contributions. We generalize the linear bias approximation to relate the observed galaxy fluctuation field to the underlying matter distribution in a gauge-invariant way. Our full formalism is essential for the consistency of theoretical predictions. As our first application, we compute the angular auto correlation of large-scale structure and its cross correlation with CMB temperature anisotropies. We comment on the possibility of detecting primordial gravity waves using galaxy clustering and discuss further applications of our formalism.
C1 [Yoo, Jaiyul; Zaldarriaga, Matias] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fitzpatrick, A. Liam] Boston Univ, Dept Phys, Boston, MA 02215 USA.
[Zaldarriaga, Matias] Harvard Univ, Jefferson Phys Lab, Cambridge, MA 02138 USA.
[Zaldarriaga, Matias] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA.
RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jyoo@cfa.harvard.edu
FU Department of Energy [DE-FG02-01ER-40676]; David and Lucile Packard
Foundation; Alfred P. Sloan Foundation; John D. and Catherine T.
MacArthur Foundation; NSF [AST05-06556]; NASA [NNG 05GJ40G]
FX We acknowledge useful discussions with Daniel Baumann, Antony Lewis,
Jordi Miralda-Escude, Jonathan Pritchard, and Anze Slosar. J.Y. is
supported by the Harvard College Observatory under the Donald H. Menzel
fund. A. L. F. is supported by the Department of Energy Grant No.
DE-FG02-01ER-40676. M. Z. is supported by the David and Lucile Packard,
the Alfred P. Sloan, and the John D. and Catherine T. MacArthur
Foundations. This work was further supported by NSF Grant No.
AST05-06556 and NASA ATP Grant No. NNG 05GJ40G.
NR 36
TC 104
Z9 104
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT
PY 2009
VL 80
IS 8
AR 083514
DI 10.1103/PhysRevD.80.083514
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 513WB
UT WOS:000271353700029
ER
PT J
AU Cernusak, LA
Winter, K
Turner, BL
AF Cernusak, Lucas A.
Winter, Klaus
Turner, Benjamin L.
TI Physiological and isotopic (delta C-13 and delta O-18) responses of
three tropical tree species to water and nutrient availability
SO PLANT CELL AND ENVIRONMENT
LA English
DT Article
DE carbon isotope ratio; leaf N concentration; oxygen isotope ratio;
transpiration; tropical tree; water-use efficiency
ID STABLE CARBON ISOTOPES; MOENCH VOSS SEEDLINGS; WHOLE-PLANT WATER; USE
EFFICIENCY; LEAF WATER; TRANSPIRATION EFFICIENCY; STOMATAL CONDUCTANCE;
CONCEPTUAL-MODEL; FICUS-INSIPIDA; COTTON LEAVES
AB Water-use efficiency and stable isotope composition were studied in three tropical tree species. Seedlings of Tectona grandis, Swietenia macrophylla and Platymiscium pinnatum were grown at either high or low water supply, and with or without added fertilizer. These three species previously exhibited low, intermediate and high whole-plant water-use efficiency (TE) when grown at high water supply in unfertilized soil. Responses of TE to water and nutrient availability varied among species. The TE was calculated as experiment-long dry matter production divided by cumulative water use. Species-specific offsets were observed in relationships between TE and whole-plant C-13 discrimination (Delta C-13(p)). These offsets could be attributed to a breakdown in the relationship between Delta C-13(p) and the ratio of intercellular to ambient CO2 partial pressures (c(i)/c(a)) in P. pinnatum, and to variation among species in the leaf-to-air vapour pressure difference (v). Thus, a plot of v center dot TE against c(i)/c(a) showed a general relationship among species. Relationships between delta O-18 of stem dry matter and stomatal conductance ranged from strongly negative for S. macrophylla to no relationship for T. grandis. Results suggest inter-specific variation among tropical tree species in relationships between stable isotope ratios (delta C-13 and delta O-18) and the gas exchange processes thought to affect them.
C1 [Cernusak, Lucas A.; Winter, Klaus; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Cernusak, LA (reprint author), Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia.
EM lucas.cernusak@cdu.edu.au
RI Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011
OI Turner, Benjamin/0000-0002-6585-0722; Cernusak,
Lucas/0000-0002-7575-5526
FU Australian Research Council; Smithsonian Tropical Research Institute
FX We thank Jorge Aranda, Milton Garcia, Aurelio Virgo, Lisa Petheram,
Carlos Martinez, Tania Romero and Aneth Sarmiento for technical
assistance in carrying out the experiment. Lucas A. Cernusak was
supported by a Tupper Postdoctoral Fellowship from the Smithsonian
Tropical Research Institute and by an Australian Postdoctoral Fellowship
from the Australian Research Council.
NR 61
TC 40
Z9 42
U1 2
U2 29
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0140-7791
J9 PLANT CELL ENVIRON
JI Plant Cell Environ.
PD OCT
PY 2009
VL 32
IS 10
BP 1441
EP 1455
DI 10.1111/j.1365-3040.2009.02010.x
PG 15
WC Plant Sciences
SC Plant Sciences
GA 491PV
UT WOS:000269592300014
PM 19558409
ER
PT J
AU Meickle, T
Matthew, S
Ross, C
Luesch, H
Paul, V
AF Meickle, Theresa
Matthew, Susan
Ross, Cliff
Luesch, Hendrik
Paul, Valerie
TI Bioassay-Guided Isolation and Identification of Desacetylmicrocolin B
from Lyngbya cf. polychroa
SO PLANTA MEDICA
LA English
DT Article
DE cyanobacteria; Oscillatoriaceae; Lyngbya polychroa; microcolins;
cytotoxins
ID MICROCOLIN-A; MARINE CYANOBACTERIA; ANTIMICROBIAL ACTIVITIES;
NATURAL-PRODUCTS; ANALOGS; POTENT; SAPROPHYTES; PATHOGENS; EXTRACTS;
PLANTS
AB Bioassay-guided fractionation of a non-polar extract of Lyngbya cf. polychroa resulted in the isolation of the cytotoxic desacetylmicrocolin B (1) as well as the known compounds microcolins A (2) and B (3). Compound 1 was found to inhibit the growth of HT-29 colorectal adenocarcinoma and IMR-32 neuroblastoma cells with half maximal inhibitory concentration (IC(50)) values of 14 nM for both cancer cell types. Microcolins A and B were found to have little activity against two strains of the marine fungus Dendryphiella salina with LD(50) values above 200 mu g/mL. Compounds 1, 2, and 3 were obtained by reverse-phase chromatography and their structures were determined by NMR and MS. In this paper we report the isolation, identification, and biological activity of 1.
C1 [Meickle, Theresa; Paul, Valerie] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Meickle, Theresa] Florida Atlantic Univ, Boca Raton, FL 33431 USA.
[Matthew, Susan; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL USA.
[Ross, Cliff] Univ N Florida, Jacksonville, FL USA.
RP Paul, V (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM paul@si.edu
RI Matthew, Susan/E-3817-2012; Ross, Cliff/B-8291-2011
FU National Oceanic and Atmospheric administration's ECOHAB
[NA05NOS4781194]; NOAA; Office of Sea; U.S. Department of Commerce
[NA060AR4170014]; NIGMS [P41GM086210]
FX Funding was provided by the National Oceanic and Atmospheric
administration's ECOHAB Program (Project NA05NOS4781194), the Florida
Sea Grant College Program with support from NOAA, Office of Sea Grant,
U.S. Department of Commerce, Grant No. NA060AR4170014, and NIGMS grant
P41GM086210. We are grateful for the use of the NMR spectrometer at
Harbor Branch Oceanographic Institute at Florida Atlantic University and
gratefully acknowledge NSF for funding through the External User Program
of the National High Magnetic Field Laboratory, which supported NMR
studies at the Advanced Magnetic Resonance Imaging and Spectroscopy
facility at the University of Florida (UF). We thank Sarath Gunasekera,
who provided many helpful suggestions on this research, and Jody Johnson
for LC-MS/MS analysis (Department of Chemistry, UF). HR-MS analyses were
performed at the UCR Mass Spectrometry Facility, Department of
Chemistry, University of California at Riverside. This is contribution #
772 of the Smithsonian Marine Station of Fort Pierce.
NR 19
TC 8
Z9 8
U1 0
U2 4
PU GEORG THIEME VERLAG KG
PI STUTTGART
PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY
SN 0032-0943
J9 PLANTA MED
JI Planta Med.
PD OCT
PY 2009
VL 75
IS 13
BP 1427
EP 1430
DI 10.1055/s-0029-1185675
PG 4
WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary
Medicine; Pharmacology & Pharmacy
SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary
Medicine
GA 516XP
UT WOS:000271577000012
PM 19431099
ER
PT J
AU Mathis, WN
Knutson, LV
Murphy, WL
AF Mathis, Wayne N.
Knutson, Lloyd V.
Murphy, Willam L.
TI A NEW SPECIES OF SNAIL-KILLING FLY OF THE GENUS DICTYA MEIGEN FROM THE
DELMARVA STATES (DIPTERA: SCIOMYZIDAE)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Dictya orthi; new species; generic diagnosis; key to species
AB A new species of snail-killing fly, Dictya orthi (Diptera: Sciomyzidae), is described from the Delmarva States (type locality: Virginia. Stafford; Aquia Harbour, Lions Park). Provided are detailed photographs, descriptions of structures of the male terminalia, a generic diagnosis, and a key to species of Dictya from the Delmarva and adjacent states.
C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA.
[Knutson, Lloyd V.] Smithsonian Inst, USDA, Systemat Entomol Lab, Washington, DC 20013 USA.
RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MRC 169, Washington, DC 20013 USA.
EM mathisw@si.edu; lvknutson@tiscali.it; billmurphy8@sbcglobal.net
FU National Park Service; Williston Fund (Smithsonian Institution)
FX We gratefully acknowledge the assistance and cooperation of many
individuals who contributed to the field work and production of this
paper. Field work in the George Washington Memorial Parkway was
supported by a grant from the National Park Service; we especially thank
Brent W. Steury (National Park Service, George Washington Memorial
Parkway, 20242 Turkey Run Park, McLean, VA 22101, USA) for his
assistance, facilitation, and support. We also acknowledge the financial
support of the Williston Fund (Smithsonian Institution), especially for
study of specimens in other museums during the summers of 2007 and 2008.
We thank Karolyn Darrow (Department of Entomology, P.O. Box 37012, MRC
165; Smithsonian Institution, Washington, D.C. 20013-7012, USA) for
assisting us in making up the plate of photographs and their
enhancement. We thank Allen L. Norrbom (Systematic Entomology
Laboratory, ARS, USDA, c/o Department of Entomology, P.O. Box 37012, MRC
169; Smithsonian Institution, Washington, D.C. 20013-7012, USA), Stephen
D. Gaimari (Department of Food and Agriculture, Plant Pest Diagnostics
Branch, 3294 Meadowview Road, Sacramento, CA 95832-1448, USA), and Karl
R. Valley (Division of Plant Protection, Bureau of Plant Industry,
Pennsylvania Department of Agriculture, Harrisburg, PA 17110, USA) for
reviewing a draft of this paper.
NR 16
TC 3
Z9 3
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2009
VL 111
IS 4
BP 785
EP 794
DI 10.4289/0013-8797-111.4.785
PG 10
WC Entomology
SC Entomology
GA 515FQ
UT WOS:000271453600003
ER
PT J
AU Pereira, AIA
Smith, DR
Zanuncio, JC
Serrao, JE
AF Pereira, Alexandre I. A.
Smith, David R.
Zanuncio, Jose C.
Serrao, Jose E.
TI LIFE HISTORY NOTES ON THE SAWFLY HAPLOSTEGUS NIGRICRUS CONDE
(HYMENOPTERA: PERGIDAE) ON PSIDIUM GUAJAVA (MYRTACEAE) IN MINAS GERAIS
STATE, BRAZIL
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE sawfly; guava; Symphyta; herbivory
ID BIOLOGICAL-CONTROL AGENT; SMITH HYMENOPTERA; HOST-SPECIFICITY; BEHAVIOR;
TENTHREDINIDAE; OVIPOSITION; ALLOCATION; PREDATION; SYMPHYTA; ARGIDAE
AB The life history of Haplostegus nigricrus Conde (Hymenoptera: Pergidae), a leaf-feeding sawfly of Psidium guajava L. (Myrtaceae), was studied in Vicosa, Minas Gerais State, Brazil. The life history and morphology are compared with those of Haplostegus epimelas Konow (Hymenoptera: Pergidae), another species that feeds on guava leaves. Haplostegus nigricrus females oviposit in the midrib of guava, and larvae feed on the leaves. Late-instar larvae drop to the ground and construct a cell for pupation. Cocoons are made individually with soil particles and other substrate. Three occurrence peaks of female adults were observed for H. nigricrus and two for H. epimelas. No males of H. nigricrus were found. The importance of this study to the knowledge of South American Pergidae is discussed.
C1 [Pereira, Alexandre I. A.; Zanuncio, Jose C.] Univ Fed Vicosa, Dept Biol Anim, BIOAGRO, BR-36571000 Vicosa, MG, Brazil.
[Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Serrao, Jose E.] Univ Fed Vicosa, Dept Biol Geral, BR-36571000 Vicosa, MG, Brazil.
RP Pereira, AIA (reprint author), Univ Fed Vicosa, Dept Biol Anim, BIOAGRO, BR-36571000 Vicosa, MG, Brazil.
EM aiapereira@yahoo.com.br; dave.smith@ars.usda.gov; zanuncio@ufv.br;
jeserrao@ufv.br
RI Serrao, Jose Eduardo/H-2935-2012
FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq);
Fundacao de Amparo a Pesquisa do Estado de Minas Gerais (FAPEMIG);
Systematic Entomolology Laboratory, USDA, Washington, DC
FX We appreciate the help of the "Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico (CNPq)" and "Fundacao de Amparo a Pesquisa do
Estado de Minas Gerais (FAPEMIG)" for financial support. M. W. Gates,
Systematic Entomolology Laboratory, USDA, Washington, DC, identified the
encyrtid parasitoid. We thank T. J. Henry, Systematic Entomology
Laboratory; USDA, Washington, DC; A. Shinohara, National Museum of
Nature and Science, Tokyo; and an anonymous reviewer for helpful
comments.
NR 32
TC 1
Z9 1
U1 1
U2 3
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2009
VL 111
IS 4
BP 795
EP 806
DI 10.4289/0013-8797-111.4.795
PG 12
WC Entomology
SC Entomology
GA 515FQ
UT WOS:000271453600004
ER
PT J
AU Rota, J
Yang, A
Brown, JW
AF Rota, Jadranka
Yang, April
Brown, John W.
TI VARIATION IN THE FEMALE FRENULUM IN TORTRICIDAE (LEPIDOPTERA). PART 2.
OLETHREUTINAE
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Bactrini; Enarmoniini; Endotheniini; Eucosmini; Gatesclarkeanini;
Grapholitini; Microcorsini; morphological character; Olethreutini;
phylogeny
ID LEPIDOPTERA
AB This paper, treating the tortricid subfamily Olethreutinae, represents the second in a proposed three-part series examining variation in the number of bristles in the frenulum of female tortricid moths. Based on an examination of 6,333 individuals of 1,464 species representing 188 genera of Olethreutinae, the number of bristles in the female frenulum varies from one to six, and it is sometimes asymmetrical on the same specimen (7.5% of individuals examined). A three-bristled frenulum is the most common condition in Microcorsini, Endotheniini, Bactrini, Gatesclarkeanini, Olethreutini, Enarmoniini, and Eucosmini, with varying degrees of intraspecific variation in number within each tribe. However, in both Eucosmini and Enarmoniini several genera have a predominantly or exclusively two-bristled frenulum (e.g., Gypsonoma Meyrick, Herpystis Meyrick, and Rhopalovalva Kuznetsov in Eucosmini; Hystrichophora Walsingham, Neoanathamna Kawabe, and Pseudacroclita Oku in Enarmoniini). In Grapholitini, two- and three-bristled frenula occur in nearly equal frequency, suggesting that this character may be of some phylogenetic significance, but an overall pattern is not immediately obvious. In contrast to the situation in Chlidanotinae, where the distribution of the two- and three-bristled frenulum corroborates previously proposed phylogenetic hypotheses, we conclude that variation in the number of bristles in the frenulum in Olethreutinae is not phylogenetically informative at higher levels (e.g., tribes, subtribes) owing to the high degree of intrageneric and intraspecific variation. However, the number of bristles may be of phylogenetic significance at the generic level, particularly in Eucosmini and Grapholitini.
C1 [Rota, Jadranka] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
[Yang, April] Univ Calif Berkeley, Dept Mol & Environm Biol, Div Organisms & Environm, Berkeley, CA 94720 USA.
[Brown, John W.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Rota, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA.
EM rotaj@si.edu; lirpa.gnay@gmail.com; john.brown@ars.usda.gov
RI Rota, Jadranka/C-6702-2011
OI Rota, Jadranka/0000-0003-0220-3920
FU Smithsonian Institution Women's Committee; Smithsonian Institution
Postdoctoral Fellowship
FX The Smithsonian Institution Women's Committee provided funding for a
Research Training Program internship for April Yang, during which some
of the data were captured. Data capture, analyses, and manuscript
preparation by Jadranka Rota was funded in part by a Smithsonian
Institution Postdoctoral Fellowship. The following provided helpful
reviews of the manuscript: Leif Aarvik, Natural History Museum, Oslo;
and Robert Kula and Thomas Henry, Systematic Entomology Laboratory,
USDA, National Museum of Natural History, Washington, D.C. We also thank
two anonymous reviewers, one of whom provided suggestions that
considerably improved the clarity of the manuscript.
NR 14
TC 3
Z9 3
U1 0
U2 3
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2009
VL 111
IS 4
BP 826
EP 866
DI 10.4289/0013-8797-111.4.826
PG 41
WC Entomology
SC Entomology
GA 515FQ
UT WOS:000271453600006
ER
PT J
AU Smith, DR
Schmidt, S
AF Smith, David R.
Schmidt, Stefan
TI REDISCOVERY OF THE PERREYIINE GENUS BARILOCHIA MALAISE (HYMENOPTERA:
PERGIDAE) IN SOUTH AMERICA
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE sawflies; new species; Chile
AB The sawfly genus Barilochia Malaise (Pergidae: Perreyiinae) was known from a single specimen of one species, B. brunneovirens Malaise, from San Carlos de Bariloche, Rio Negro, Argentina. A second species from Chile, B. longivalvula, n. sp., is described and illustrated. A male of Barilochia is described for the first time. The possible host plant is Nothofagus dombeyi (Coihue) (Nothofagaceae).
C1 [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Schmidt, Stefan] Zool Staatssammlung Munchen, D-81247 Munich, Germany.
RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 73012,MRC 168, Washington, DC 20013 USA.
EM dave.smith@ars.usda.gov; stefan.schmidt@zsm.mnw.de
NR 5
TC 0
Z9 0
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2009
VL 111
IS 4
BP 874
EP 879
DI 10.4289/0013-8797-111.4.874
PG 6
WC Entomology
SC Entomology
GA 515FQ
UT WOS:000271453600008
ER
PT J
AU Perez-Gelabert, DE
AF Perez-Gelabert, Daniel E.
TI Synonymy in Caribbean Tetrigidae (Orthoptera)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Editorial Material
C1 Smithsonian Inst, US Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Perez-Gelabert, DE (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA.
EM perezd@si.edu
NR 2
TC 0
Z9 0
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2009
VL 111
IS 4
BP 900
EP 901
DI 10.4289/0013-8797-111.4.900
PG 2
WC Entomology
SC Entomology
GA 515FQ
UT WOS:000271453600012
ER
PT J
AU Sanchez-Azofeifa, GA
Castro, K
Wright, SJ
Gamon, J
Kalacska, M
Rivard, B
Schnitzer, SA
Feng, JL
AF Arturo Sanchez-Azofeifa, G.
Castro, Karen
Joseph Wright, S.
Gamon, John
Kalacska, Margaret
Rivard, Benoit
Schnitzer, Stefan A.
Feng, Ji Lu
TI Differences in leaf traits, leaf internal structure, and spectral
reflectance between two communities of lianas and trees: Implications
for remote sensing in tropical environments
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Tropical dry forests; Tropical rainforest; Spectroscopy; Liana leaves;
Tree leaves; Pigment concentration; Internal leaf structure;
Hyperspectral remote sensing
ID BARRO-COLORADO ISLAND; EXTREME-SHADE PLANTS; DRY FOREST LIANAS;
OPTICAL-PROPERTIES; HYPERSPECTRAL DATA; CANOPY; PANAMA; DISCRIMINATION;
NUTRIENT; AREA
AB Increasing dominance of lianas in many tropical forests is considered a fingerprint of global environmental change. Despite the key role they play in ecosystem functioning, lianas remain one of the least studied life forms in tropical environments. This paper contrasts leaf traits and spectral properties (400-1100 nm) of liana and tree communities from a tropical dry forest and a tropical rainforest in Panama, Central America. Differences between lianas and tree leaf traits were analyzed using spectroscopy, leaf histology and pigment extractions. Results from this study indicate that many of the biochemical, structural, and optical properties of lianas and trees are different in the dry forest site but not in rainforest sites. In the dry forest site, liana leaves exhibited significantly lower chlorophyll and carotenoid contents and were thinner than the leaves of their host trees. Specific leaf area, dry to fresh mass ratio, and mean water content of liana leaves were significantly higher when compared with tree leaves. The differences observed in the tropical dry forest site indicate that lianas may have a higher rate of resource acquisition and usage, whereas trees tend to conserve acquired resources. We suggest that our results may be indicative of the presence of a liana syndrome related to water availability and thus best exhibited in tropical dry forests. Our findings have important implications for using remote sensing to accurately map the distribution of liana communities at regional scales and for the continued expansion of lianas in tropical environments as a result of global change. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Arturo Sanchez-Azofeifa, G.; Castro, Karen; Gamon, John; Rivard, Benoit; Feng, Ji Lu] Univ Alberta, Dept Earth & Atmospher Sci, EOSL, Edmonton, AB T6G 2E3, Canada.
[Arturo Sanchez-Azofeifa, G.; Joseph Wright, S.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Kalacska, Margaret] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada.
[Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA.
RP Sanchez-Azofeifa, GA (reprint author), Univ Alberta, Dept Earth & Atmospher Sci, EOSL, Edmonton, AB T6G 2E3, Canada.
EM arturo.sanchez@ualberta.ca
RI Gamon, John/A-2641-2014; Wright, Stuart/M-3311-2013;
OI Gamon, John/0000-0002-8269-7723; Wright, Stuart/0000-0003-4260-5676;
Schnitzer, Stefan/0000-0002-2715-9455; Kalacska,
Margaret/0000-0002-1676-481X
FU Smithsonian Tropical Research Institute; Natural Sciences and
Engineering Research Council of Canada; Inter American Institute for
Global Change Research Collaborative Research Network [CRN2-021]; U.S.
National Science Foundation [GEO-0452325]
FX We thank the help of Mima Samarniego who provided important insights on
species identification at both tropical canopy cranes in Panama. The
Smithsonian Tropical Research Institute, the Natural Sciences and
Engineering Research Council of Canada (Discovery grant program), and
the Inter American Institute for Global Change Research Collaborative
Research Network (CRN2-021) program that is supported by the U.S.
National Science Foundation (Grant GEO-0452325) supported this work. We
also want to thank the suggestions and comments from three anonymous
reviewers.
NR 59
TC 39
Z9 41
U1 7
U2 60
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD OCT
PY 2009
VL 113
IS 10
BP 2076
EP 2088
DI 10.1016/j.rse.2009.05.013
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 487MA
UT WOS:000269277200004
ER
PT J
AU Zhao, YH
Huang, JS
Ashby, M
Fazio, G
Miyazaki, S
AF Zhao, Ying-He
Huang, Jia-Sheng
Ashby, Matthew
Fazio, Giovanni
Miyazaki, Satoshi
TI The deep optical imaging of the Extended Groth Strip
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE galaxies: high-redshift; galaxies: photometry; surveys
ID GALAXY NUMBER COUNTS; LYMAN-BREAK GALAXIES; SPITZER-SPACE-TELESCOPE;
STAR-FORMING GALAXIES; LY-ALPHA SYSTEMS; FAINT GALAXIES; MIDINFRARED
OBSERVATIONS; PHOTOMETRIC SELECTION; CCD OBSERVATIONS; STELLAR MASSES
AB We present u',g' R optical images taken with the MMT/Megacam and the Subaru/Suprime telescopes of the Extended Groth Strip survey. The total survey covers an area of about similar to 1 degree(2), including four sub-fields and is optimized for the study of galaxies at z similar to 3. Our methods for photometric calibration in AB magnitudes, the limiting magnitude and the galaxy number count are described. A sample of 1642 photometrically selected candidate Lyman-Break Galaxies (LBGs) to an apparent R(AB) magnitude limit of 25.0 is presented. The average sky surface density of our LBG sample is similar to 1.0 arcmin(-2), slightly higher than the previous finding.
C1 [Zhao, Ying-He] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Zhao, Ying-He; Huang, Jia-Sheng; Ashby, Matthew; Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zhao, Ying-He] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Miyazaki, Satoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Zhao, YH (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
EM yhzhao@pmo.ac.cn
FU China Scholarship Council (CSC); Jiangsu Planned Projects for
Postdoctoral Research Funds [0802031C]; K.C. Wong Education Foundation,
Hong Kong
FX The observations reported here were obtained in part at the MMT
Observatory, a facility operated jointly by the Smithsonian Institution
and the University of Arizona. Y. H. ZHAO would like to gratefully
acknowledge financial support from the China Scholarship Council (CSC),
the Jiangsu Planned Projects for Postdoctoral Research Funds (No.
0802031C) and the K.C. Wong Education Foundation, Hong Kong.
NR 65
TC 5
Z9 5
U1 0
U2 2
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD OCT
PY 2009
VL 9
IS 10
BP 1061
EP 1077
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 512QX
UT WOS:000271266300001
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI FROM THE CASTLE Mind-Meld
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD OCT
PY 2009
VL 40
IS 7
BP 24
EP 24
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 503VB
UT WOS:000270567800010
ER
PT J
AU Hacker, BC
AF Hacker, Barton C.
TI Disrupting Science: Social Movements, American Scientists, and the
Politics of the Military, 1945-1975.
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 [Hacker, Barton C.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4363 USA
SN 0040-165X
EI 1097-3729
J9 TECHNOL CULT
JI Technol. Cult.
PD OCT
PY 2009
VL 50
IS 4
SI SI
BP 947
EP 949
PG 3
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 518SA
UT WOS:000271712200026
ER
PT J
AU Mastin, LG
Guffanti, M
Servranckx, R
Webley, P
Barsotti, S
Dean, K
Durant, A
Ewert, JW
Neri, A
Rose, WI
Schneider, D
Siebert, L
Stunder, B
Swanson, G
Tupper, A
Volentik, A
Waythomas, CF
AF Mastin, L. G.
Guffanti, M.
Servranckx, R.
Webley, P.
Barsotti, S.
Dean, K.
Durant, A.
Ewert, J. W.
Neri, A.
Rose, W. I.
Schneider, D.
Siebert, L.
Stunder, B.
Swanson, G.
Tupper, A.
Volentik, A.
Waythomas, C. F.
TI A multidisciplinary effort to assign realistic source parameters to
models of volcanic ash-cloud transport and dispersion during eruptions
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Review
DE volcanic eruption; aircraft; volcanic plumes; ash clouds
ID TEPHRA-FALL DEPOSITS; GRAIN-SIZE DISTRIBUTION; MOUNT ST-HELENS;
KATMAI-NATIONAL-PARK; THERMAL DISEQUILIBRIUM; PARTICLE AGGREGATION;
MIYAKEJIMA VOLCANO; PLINIAN ERUPTIONS; COLUMN DYNAMICS; REDOUBT VOLCANO
AB During volcanic eruptions, volcanic ash transport and dispersion models (VATDs) are used to forecast the location and movement of ash clouds over hours to days in order to define hazards to aircraft and to communities downwind. Those models use input parameters, called "eruption source parameters", such as plume height H, mass eruption rate M, duration D, and the mass fraction m(63) oferupted debris finer than about 4 phi or 63 mu m, which can remain in the cloud for many hours or days. Observational constraints on the value of such parameters are frequently unavailable in the first minutes or hours after an eruption is detected. Moreover, observed plume height may change during an eruption, requiring rapid assignment of new parameters. This paper reports on a group effort to improve the accuracy of source parameters used by VATDs in the early hours of an eruption. We do so by first compiling a list of eruptions for which these parameters are well constrained. and then using these data to review and update previously studied parameter relationships. We find that the existing scatter in plots of H versus Myields an uncertainty within the 50% confidence interval of plus or minus a factor of four in eruption rate for a given plume height This scatter is not clearly attributable to biases in measurement techniques or to well-recognized processes such as elutriation from pyroclastic flows. Sparse data on total grain-size distribution suggest that the mass fraction of fine debris m(63) could vary by nearly two orders of magnitude between small basaltic eruptions (similar to 0.01) and large silicic ones (>0.5). We classify eleven eruption types; four types each for different sizes of silicic and mafic eruptions; submarine eruptions; "brief' or Vulcanian eruptions; and eruptions that generate co-ignimbrite or co-pyroclastic flow plumes. For each eruption type we assign source parameters. We then assign a characteristic eruption type to each of the world's similar to 1500 Holocene volcanoes. These eruption types and associated parameters can be used for ash-cloud modeling in the event of an eruption, when no observational constraints on these parameters are available. Published by Elsevier B.V.
C1 [Mastin, L. G.; Ewert, J. W.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA.
[Guffanti, M.] US Geol Survey, Reston, VA 22092 USA.
[Servranckx, R.] Canadian Meteorol Ctr, Quebec City, PQ, Canada.
[Webley, P.; Dean, K.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK USA.
[Barsotti, S.; Neri, A.] Ist Nazl Geofis & Vulcanol, Sez Pisa, Pisa, Italy.
[Durant, A.] Univ Bristol, Dept Earth Sci, Bristol BS8 1TH, Avon, England.
[Rose, W. I.] Michigan Technol Univ, Dept Geol & Engn Sci, Houghton, MI 49931 USA.
[Schneider, D.; Waythomas, C. F.] USGS Alaska Volcano Observ, Anchorage, AK USA.
[Siebert, L.] Smithsonian Inst, Washington, DC 20560 USA.
[Stunder, B.] NOAA, Air Resources Lab, Silver Spring, MD 20910 USA.
[Swanson, G.] NOAA, Camp Springs, MD USA.
[Tupper, A.] Bur Meteorol, Casuarina, NT, Australia.
[Volentik, A.] Univ S Florida, Dept Geol, Tampa, FL 33620 USA.
RP Mastin, LG (reprint author), US Geol Survey, Cascades Volcano Observ, 1300 SE Cardinal Court,Bldg 10,Suite 100, Vancouver, WA 98683 USA.
EM lgmastin@usgs.gov
RI Neri, Augusto/A-1623-2009; Wei, Jianjian/F-7788-2011; Durant,
Adam/C-7883-2014; Webley, Peter/F-8238-2015; Stunder,
Barbara/C-3106-2016
OI Neri, Augusto/0000-0002-3536-3624; Wei, Jianjian/0000-0001-8859-8462;
Durant, Adam/0000-0002-0198-7332; Webley, Peter/0000-0001-5327-8151;
NR 101
TC 201
Z9 204
U1 5
U2 60
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD SEP 30
PY 2009
VL 186
IS 1-2
BP 10
EP 21
DI 10.1016/j.jvolgeores.2009.01.008
PG 12
WC Geosciences, Multidisciplinary
SC Geology
GA 498DN
UT WOS:000270117100002
ER
PT J
AU Tupper, A
Wunderman, R
AF Tupper, Andrew
Wunderman, Rick
TI Reducing discrepancies in ground and satellite-observed eruption heights
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE volcanic ash; volcanic eruptions; volcanic clouds; natural hazards;
remote sensing; volcanic monitoring; aviation safety
ID EXPLOSIVE VOLCANIC-ERUPTIONS; DYNAMICS; ASH; FAILURES; ALASKA; CLOUD
AB The plume height represents a crucial piece of evidence about an eruption, feeding later assessment of its size, character, and potential impact, and feeding real-time warnings for aviation and ground-based populations. There have been many observed discrepancies between different observations of maximum plume height for the same eruption. A comparison of maximum daily height estimates of volcanic clouds over Indonesia and Papua New Guinea during 1982-2005 shows marked differences between ground and satellite estimates, and a general tendency towards lower height estimates from the ground. Without improvements in the quality of these estimates, reconciled among all available methods, warning systems will be less effective than they should be and the world's record of global volcanism will remain hard to quantify. Examination of particular cases suggests many possible reasons for the discrepancies. Consideration of the satellite and radar cloud observations for the 1991 Pinatubo eruptions shows that marked differences can exist even with apparently good observations. The problem can be understood largely as a sampling issue, as the most widely reported parameter. the maximum cloud height, is highly sensitive to the frequency of observation. Satellite and radar cloud heights also show a pronounced clumping near the height of the tropopause and relative lack of eruptions reaching only the mid-troposphere, reinforcing the importance of the tropopause in determining the eruption height in convectively unstable environments. To reduce the discrepancies between ground and satellite estimates, a number of formal collaboration measures between vulcanological, meteorological and aviation agencies are suggested. Crown Copyright (C) 2009 Published by Elsevier B.V. All rights reserved.
C1 [Tupper, Andrew] Bur Meteorol, Casuarina, NT 0811, Australia.
[Wunderman, Rick] Smithsonian Inst, Global Volcanism Program, Washington, DC 20013 USA.
RP Tupper, A (reprint author), Bur Meteorol, POB 40050, Casuarina, NT 0811, Australia.
EM A.Tupper@bom.gov.au; wunderma@si.edu
NR 39
TC 21
Z9 21
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD SEP 30
PY 2009
VL 186
IS 1-2
BP 22
EP 31
DI 10.1016/j.jvolgeores.2009.02.015
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA 498DN
UT WOS:000270117100003
ER
PT J
AU Harasewych, MG
Strong, EE
AF Harasewych, M. G.
Strong, Ellen E.
TI PROCEEDINGS OF THE SYMPOSIUM "NEOGASTROPOD ORIGINS, PHYLOGENY,
EVOLUTIONARY PATHWAYS AND MECHANISMS" HELD DURING THE 2007 WORLD
CONGRESS OF MALACOLOGY, ANTWERP, BELGIUM, 15-20 JULY 2007 GUEST EDITORS
MG HARASEWYCH AND ELLEN E. STRONG Preface
SO NAUTILUS
LA English
DT Editorial Material
C1 [Harasewych, M. G.; Strong, Ellen E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU BAILEY-MATTHEWS SHELL MUSEUM
PI SANIBEL
PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD,
SANIBEL, FL 33957 USA
SN 0028-1344
J9 NAUTILUS
JI Nautilus
PD SEP 28
PY 2009
VL 123
IS 3
BP 71
EP 71
PG 1
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 503HN
UT WOS:000270524400001
ER
PT J
AU Taviani, M
Angeletti, L
Dimech, M
Mifsud, C
Freiwald, A
Harasewych, MG
Oliverio, M
AF Taviani, Marco
Angeletti, Lorenzo
Dimech, Mark
Mifsud, Constantine
Freiwald, Andre
Harasewych, M. G.
Oliverio, Marco
TI Coralliophilinae (Gastropoda: Muricidae) associated with deep-water
coral banks in the Mediterranean
SO NAUTILUS
LA English
DT Article; Proceedings Paper
CT Symposium on Neogastropod Origins, Phylogeny, Evolutionary Pathways and
Mechanisms held at the World Congress of Malacology
CY JUL 15-20, 2007
CL Antwerp, BELGIUM
DE Neogastropoda; cnidaria; predation; biogeography; amphi-Atlantic;
biodiversity
ID ATLANTIC; SEA
AB Fisheries and scientific investigations of the recently discovered deep-water coral province south of Malta sampled living specimens of two deep-water Coralliophilinae intimately associated with Lophelia-Madrepora coral banks. The species are "Coralliophila" richardi (Fischer P., 1882) and Babelomurex sentix (Bayer, 1971). A third coralliophilinid "Coralliophila" squamosa (Bivona Ant. in Bivoria And., 1838: deep-water morphotype) has been also observed alive close to deep-water corals at the Nameless-Urania Bank.
C1 [Taviani, Marco; Angeletti, Lorenzo] CNR, ISMAR, I-40129 Bologna, Italy.
[Dimech, Mark] Univ Malta, St Venera, Malta.
[Freiwald, Andre] Univ Erlangen Nurnberg, GZN Geozentrum Nordbayern, Erlangen, Germany.
[Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Oliverio, Marco] Univ Roma La Sapienza, Dipartimento Biol Anim & Uomo, I-00185 Rome, Italy.
RP Taviani, M (reprint author), CNR, ISMAR, Via Gobetti 101, I-40129 Bologna, Italy.
EM marco.taviani@bo.ismar.cnr.it; lorenzo.angeletti@bo.ismar.cnr.it;
mdim@mail.global.net.mt; kejdon@orbit.net.mt;
Andre.Freiwald@gzn.uni-erlangen.de; Harasewych@si.edu;
marco.oliverio@uniroma1.it
RI OLIVERIO, MARCO/F-2229-2010; CNR, Ismar/P-1247-2014;
OI OLIVERIO, MARCO/0000-0002-0316-4364; CNR, Ismar/0000-0001-5351-1486;
Freiwald, Andre/0000-0002-2335-4042; taviani, marco/0000-0003-0414-4274
NR 32
TC 9
Z9 9
U1 0
U2 8
PU BAILEY-MATTHEWS SHELL MUSEUM
PI SANIBEL
PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD,
SANIBEL, FL 33957 USA
SN 0028-1344
J9 NAUTILUS
JI Nautilus
PD SEP 28
PY 2009
VL 123
IS 3
BP 106
EP 112
PG 7
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 503HN
UT WOS:000270524400005
ER
PT J
AU Baeza, JA
Bolanos, JA
Hernandez, JE
Lopez, R
AF Antonio Baeza, J.
Bolanos, Juan A.
Hernandez, Jesus E.
Lopez, Regulo
TI A new species of Lysmata (Crustacea, Decapoda, Hippolytidae) from
Venezuela, southeastern Caribbean Sea
SO ZOOTAXA
LA English
DT Article
DE Lysmata; Lysmatidae; Hippolytidae; Caribbean; Venezuela; hermaphrodite
ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; MARINE SHRIMP; WURDEMANNI
CARIDEA; WESTERN ATLANTIC; ALLOCATION
AB Lysmata udoi n. sp., a new peppermint shrimp, is described from Venezuela, southeastern Caribbean Sea. All individuals were collected from dens of the toadfish Amphichthys criptocentrus (Valenciennes, 1837) in the subtidal zone. This new species can be distinguished from other closely related species of Lysmata by the number of teeth, length and shape of the rostrum, the relative length of the antennular peduncle, and the number of carpal articles of the second pereiopod. The color pattern is distinctive. The fourth abdominal segment almost lacks color, but bears a posterior red thin line with three short forward projections. Morphological and molecular characters demonstrate that L. udoi n. sp. is most closely related to the Gulf of Mexico L. boggessi Rhyne and Lin, 2006 and the Caribbean L. rafa Rhyne and Anker, 2007 and L. ankeri Rhyne and Lin, 2006. Field observations suggest that L. udoi n. sp. is a protandric simultaneous hermaphrodite, with a primary male phase followed by a simultaneous hermaphrodite phase.
C1 [Antonio Baeza, J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
[Bolanos, Juan A.; Hernandez, Jesus E.; Lopez, Regulo] Univ Oriente, Nucleo Nueva Esparta, Escuela Ciencias Aplicadas Mar, Grp Invest Carcinol, Isla Margarita, Venezuela.
RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
EM baezaa@si.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
FU Smithsonian Tropical Research Institute (STRI) Marine Fellowship;
Smithsonian Marine Station (Fort Pierce, Florida) Fellowship
FX JAB appreciates the support from the Smithsonian Tropical Research
Institute (STRI) Marine Fellowship and the Smithsonian Marine Station
(Fort Pierce, Florida) Fellowship. Support for research from the Consejo
de Investigacion, Universidad de Oriente, Venezuela is deeply
appreciated. Especial thanks to Jeff Hunt and Lee Weigt at the
Laboratory of Analytical Biology, NMNH, Washington D. C. for their
logistical support. Two anonymous reviewers helped improve previous
versions of the present manuscript. This is contribution number 801 from
the Smithsonian Marine Station at Fort Pierce.
NR 26
TC 7
Z9 11
U1 0
U2 2
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD SEP 25
PY 2009
IS 2240
BP 60
EP 68
PG 9
WC Zoology
SC Zoology
GA 498WN
UT WOS:000270176500004
ER
PT J
AU Kwan, JC
Eksioglu, EA
Liu, C
Paul, VJ
Luesch, H
AF Kwan, Jason C.
Eksioglu, Erika A.
Liu, Chen
Paul, Valerie J.
Luesch, Hendrik
TI Grassystatins A-C from Marine Cyanobacteria, Potent Cathepsin E
Inhibitors That Reduce Antigen Presentation
SO JOURNAL OF MEDICINAL CHEMISTRY
LA English
DT Article
ID CRYSTAL-STRUCTURE; ASPARTIC PROTEINASE; CRYSTALLOGRAPHIC ANALYSIS;
PEPSTATIN-A; SYMPLOCA SP; SUBSTRATE-SPECIFICITY; COUPLING-CONSTANTS;
CONTAINING PEPTIDE; 1.8-A RESOLUTION; PEPSIN INHIBITOR
AB In our efforts to explore marine cyanobacteria as a source of novel bioactive compounds, we discovered a statine unit-containing linear decadepsipeptide, grassystatin A (1), which we screened against a diverse set of 59 proteases. We describe the structure determination of I and two natural analogues, grassystatins B (2) and C (3), using NMR, MS, and chiral HPLC techniques. Compound I selectively inhibited cathepsins D and E with IC(50)S of 26.5 nM and 886 pM, respectively. Compound 2 showed similar potency and selectivity against cathepsins D and E (IC(50)S of 7.27 nM and 354 pM, respectively), whereas the truncated peptide analogue grassystatin C (3), which consists of two fewer residues than I and 2, was less potent against both but still selective for cathepsin E. The selectivity of compounds 1-3 for cathepsin E over D (20-38-fold) suggests that these natural products may be useful tools to probe cathepsin E function. We investigated the structural basis of this selectivity using molecular docking. We also show that I can reduce antigen presentation by dendritic cells, a process thought to rely on cathepsin E.
C1 [Kwan, Jason C.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.
[Eksioglu, Erika A.; Liu, Chen] Univ Florida, Dept Pathol Immunol & Lab Med, Gainesville, FL 32610 USA.
[Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.
EM luesch@cop.ufl.edu
RI Kwan, Jason/F-9589-2010
OI Eksioglu, Erika/0000-0003-4458-7192; Kwan, Jason/0000-0001-9933-1536
FU National Institutes of Health; NIGMS [P41GM-086210]; University of
Florida College of Pharmacy; NSF; National High Magnetic Field
Laboratory (NHMFL)
FX This research was supported by the National Institutes of Health, NIGMS
Grant P41GM-086210, and the University of Florida College of Pharmacy.
We acknowledge the NSF for funding through the External User Program of
the National High Magnetic Field Laboratory (NHMFL), which supported
initial NMR studies at the Advanced Magnetic Resonance Imaging and
Spectroscopy (AMRIS) facility in the McKnight Brain Institute of the
University of Florida (UF). The 600 MHz 1 mm tripleresonance HTS
cryogenic probe used for NMR of compound I in DMSO-d6 and 3
in CDCl3 was developed through collaboration between UF,
NHMFL, and Bruker Biospin. We thank J.R. Rocca (UF) and K. Horiuchi
(RBC) for technical assistance. This is contribution 793 from the
Smithsonian Marine Station.
NR 65
TC 37
Z9 37
U1 1
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0022-2623
J9 J MED CHEM
JI J. Med. Chem.
PD SEP 24
PY 2009
VL 52
IS 18
BP 5732
EP 5747
DI 10.1021/jm9009394
PG 16
WC Chemistry, Medicinal
SC Pharmacology & Pharmacy
GA 493OJ
UT WOS:000269746600019
PM 19715320
ER
PT J
AU Thureau, ND
Monnier, JD
Traub, WA
Millan-Gabet, R
Pedretti, E
Berger, JP
Garcia, MR
Schloerb, FP
Tannirkulam, AK
AF Thureau, N. D.
Monnier, J. D.
Traub, W. A.
Millan-Gabet, R.
Pedretti, E.
Berger, J. -P.
Garcia, M. R.
Schloerb, F. P.
Tannirkulam, A. -K.
TI Imaging the asymmetric dust shell around CI Cam with long baseline
optical interferometry
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: high angular resolution; techniques: interferometric;
circumstellar matter; stars: individual: CI Cam
ID HERBIG AE/BE STARS; X-RAY TRANSIENT; SPECTROSCOPIC OBSERVATIONS; IOTA
INTERFEROMETER; CAMELOPARDALIS; EMISSION; OUTBURST; PHOTOMETRY;
J0421+560; OBJECTS
AB We present the first high angular resolution observation of the B[e] star/X-ray transient object CI Cam, performed with the two-telescope Infrared Optical Telescope Array (IOTA), its upgraded three-telescope version (IOTA3T) and the Palomar Testbed Interferometer (PTI). Visibilities and closure phases were obtained using the IONIC-3 integrated optics beam combiner. CI Cam was observed in the near-infrared H and K spectral bands, wavelengths well suited to measure the size and study the geometry of the hot dust surrounding CI Cam. The analysis of the visibility data over an 8 yr period from soon after the 1998 outburst to 2006 shows that the dust visibility has not changed over the years. The visibility data show that CI Cam is elongated which confirms the disc-shape of the circumstellar environment and totally rules out the hypothesis of a spherical dust shell. Closure phase measurements show direct evidence of asymmetries in the circumstellar environment of CI Cam and we conclude that the dust surrounding CI Cam lies in an inhomogeneous disc seen at an angle. The near-infrared dust emission appears as an elliptical skewed Gaussian ring with a major axis a = 7.58 +/- 0.24 mas, an axis ratio r = 0.39 +/- 0.03 and a position angle theta = 35 degrees +/- 2 degrees.
C1 [Thureau, N. D.; Pedretti, E.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Monnier, J. D.; Tannirkulam, A. -K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Millan-Gabet, R.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA.
[Berger, J. -P.] LAOG, Grenoble, France.
[Garcia, M. R.] Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Schloerb, F. P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Thureau, ND (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
EM nt15@st-andrews.ac.uk
FU European Community's through an International Outgoing Marie-Curie [OIF
- 002990]; Centre National de Recherche Scientifique (CNRS, France);
Centre National d'Etudes Spatiales (CNES, France); Ohio State
University; MDM consortium; MIT; NSF [AST-9605012]; Michelson
Postdoctoral Fellowship; Scottish Universities Physics Association
(SUPA); NASA [NAS8-03060]
FX M. R. Garcia acknowledges partial support from NASA Contract NAS8-03060
to the Chandra X-ray Center.
NR 45
TC 10
Z9 10
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 21
PY 2009
VL 398
IS 3
BP 1309
EP 1316
DI 10.1111/j.1365-2966.2009.14949.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493JB
UT WOS:000269731500020
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Bautista, M
Beilicke, M
Benbow, W
Boltuch, D
Bradbury, SM
Buckley, JH
Bugaev, V
Butt, Y
Byrum, K
Cannon, A
Cesarini, A
Chow, YC
Ciupik, L
Cogan, P
Cui, W
Dickherber, R
Ergin, T
Fegan, SJ
Finley, JP
Fortin, P
Fortson, L
Furniss, A
Gall, D
Gillanders, GH
Gotthelf, EV
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Horan, D
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McCann, A
McCutcheon, M
Millis, J
Moriarty, P
Mukherjee, R
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Schroedter, M
Sembroski, GH
Smith, AW
Steele, D
Swordy, SP
Theiling, M
Toner, JA
Vassiliev, VV
Vincent, S
Wagner, RG
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wissel, S
Wood, M
Zitzer, B
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Bautista, M.
Beilicke, M.
Benbow, W.
Boltuch, D.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Butt, Y.
Byrum, K.
Cannon, A.
Cesarini, A.
Chow, Y. C.
Ciupik, L.
Cogan, P.
Cui, W.
Dickherber, R.
Ergin, T.
Fegan, S. J.
Finley, J. P.
Fortin, P.
Fortson, L.
Furniss, A.
Gall, D.
Gillanders, G. H.
Gotthelf, E. V.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Horan, D.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McCann, A.
McCutcheon, M.
Millis, J.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Schroedter, M.
Sembroski, G. H.
Smith, A. W.
Steele, D.
Swordy, S. P.
Theiling, M.
Toner, J. A.
Vassiliev, V. V.
Vincent, S.
Wagner, R. G.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wissel, S.
Wood, M.
Zitzer, B.
TI DETECTION OF EXTENDED VHE GAMMA RAY EMISSION FROM G106.3+2.7 WITH
VERITAS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma rays: observations; ISM: individual (G106.3+2.7=VER J2227+608);
pulsars: individual (J2229+6114); supernova remnants
ID PULSAR WIND NEBULAE; SOURCE 3EG J2227+6122; GALACTIC-PLANE SURVEY;
SUPERNOVA REMNANT; MOLECULAR CLOUDS; SOURCE LIST; TELESCOPE; DISCOVERY;
ASTRONOMY; FIELD
AB We report the detection of very-high-energy (VHE) gamma-ray emission from supernova remnant (SNR) G106.3+2.7. Observations performed in 2008 with the VERITAS atmospheric Cherenkov gamma-ray telescope resolve extended emission overlapping the elongated radio SNR. The 7.3 sigma (pre-trials) detection has a full angular extent of roughly 0 degrees.6 by 0 degrees.4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident (12)CO (J = 1-0) emission, 0 degrees.4 away from the pulsar PSR J2229+6114, situated at the northern end of the SNR. Evidently the current-epoch particles from the pulsar wind nebula are not participating in the gamma-ray production. The VHE energy spectrum measured with VERITAS is well characterized by a power law dN/dE = N(0)(E/3 TeV)(-Gamma) with a differential index of Gamma = 2.29 +/- 0.33(stat) +/- 0.30(sys) and a flux of N(0) = (1.15 +/- 0.27(stat) +/- 0.35(sys)) x 10(-13) cm(-2) s(-1) TeV(-1). The integral flux above 1 TeV corresponds to similar to 5 percent of the steady Crab Nebula emission above the same energy. We describe the observations and analysis of the object and briefly discuss the implications of the detection in a multiwavelength context.
C1 [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Acciari, V. A.; Benbow, W.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Arlen, T.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Fortin, P.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
RP Aliu, E (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM ealiu@bartol.udel.edu; wakely@uchicago.edu
OI Lang, Mark/0000-0003-4641-4201; Cui, Wei/0000-0002-6324-5772; Cesarini,
Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel,
Dirk/0000-0003-2085-5586
FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian
Institution; Natural Sciences and Engineering Research Council (NSERC)
in Canada; Science Foundation Ireland; Science and Technology Facilities
Council in the UK
FX This research is supported by grants from the U.S. Department of Energy,
the U.S. National Science Foundation and the Smithsonian Institution, by
the Natural Sciences and Engineering Research Council (NSERC) in Canada,
by Science Foundation Ireland, and by the Science and Technology
Facilities Council in the UK. The research presented in this paper has
used data from the Canadian Galactic Plane Survey, a Canadian project
with international partners, supported by NSERC. We acknowledge the work
of the technical support staff at the FLWO, of BtWD, and of the
collaborating institutions in the construction and operation of the
instrument.
NR 44
TC 17
Z9 17
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2009
VL 703
IS 1
BP L6
EP L9
DI 10.1088/0004-637X/703/1/L6
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AQ
UT WOS:000269626600002
ER
PT J
AU Rea, N
McLaughlin, MA
Gaensler, BM
Slane, PO
Stella, L
Reynolds, SP
Burgay, M
Israel, GL
Possenti, A
Chatterjee, S
AF Rea, N.
McLaughlin, M. A.
Gaensler, B. M.
Slane, P. O.
Stella, L.
Reynolds, S. P.
Burgay, M.
Israel, G. L.
Possenti, A.
Chatterjee, S.
TI DISCOVERY OF EXTENDED X-RAY EMISSION AROUND THE HIGHLY MAGNETIC RRAT
J1819-1458
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: individual (RRAT J1819-1458); stars: magnetic fields; X-rays:
stars
ID RADIO TRANSIENT J1819-1458; PULSAR WIND NEBULAE; SUPERNOVA REMNANT;
NEUTRON-STARS; KES-75
AB We report on the discovery of extended X-ray emission around the high magnetic field rotating radio transient J1819-1458. Using a 30 ks Chandra ACIS-S observation, we found significant evidence for extended X-ray emission with a peculiar shape: a compact region out to similar to 5.'' 5, and more diffuse emission extending out to similar to 13 '' from the source. The most plausible interpretation is a nebula somehow powered by the pulsar, although the small number of counts prevents a conclusive answer on the nature of this emission. RRAT J1819-1458's spin-down energy loss rate ((E) over dot(rot) similar to 3 x 10(32) erg s(-1)) is much lower than that of other pulsars with observed spin-down-powered pulsar wind nebulae (PWNe), and implies a rather high X-ray efficiency of eta(X) equivalent to L(pwn; 0.5-8 keV)/(E) over dot(rot) similar to 0.2 at converting spin-down power into the PWNX-ray emission. This suggests the need of an additional source of energy rather than the spin-down power alone, such as the high magnetic energy of this source. Furthermore, this Chandra observation allowed us to refine the positional accuracy of RRAT J1819-1458 to a radius of similar to 0.'' 3, and confirms the presence of X-ray pulsations and the similar to 1 keV absorption line, previously observed in the X-ray emission of this source.
C1 [Rea, N.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Rea, N.] CSIC, IEEC, Inst Ciencies Espai, Fac Ciencies, Barcelona 08193, Spain.
[McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26501 USA.
[McLaughlin, M. A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Slane, P. O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stella, L.; Israel, G. L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Reynolds, S. P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Burgay, M.; Possenti, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Chatterjee, S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Chatterjee, S.] Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
RP Rea, N (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904,Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
EM n.rea@uva.nl
RI Gaensler, Bryan/F-8655-2010; Rea, Nanda/I-2853-2015;
OI Rea, Nanda/0000-0003-2177-6388; Burgay, Marta/0000-0002-8265-4344;
Israel, GianLuca/0000-0001-5480-6438; Gaensler,
Bryan/0000-0002-3382-9558
FU NWO Veni Fellowship; WVEPSCoR; SAO guest investigator grant
FX We thank T. Aldcroft and P. Plucinsky for checking the Chandra aspect
reconstruction during this observation and for useful suggestions, and
K. Borkowski, O. Kargaltsev, and P. Esposito for comments. N. R.
acknowledges support from an NWO Veni Fellowship. M. A. M. is supported
by a WVEPSCoR grant, and an SAO guest investigator grant.
NR 26
TC 28
Z9 29
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2009
VL 703
IS 1
BP L41
EP L45
DI 10.1088/0004-637X/703/1/L41
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AQ
UT WOS:000269626600010
ER
PT J
AU Breech, B
Matthaeus, WH
Cranmer, SR
Kasper, JC
Oughton, S
AF Breech, B.
Matthaeus, W. H.
Cranmer, S. R.
Kasper, J. C.
Oughton, S.
TI Electron and proton heating by solar wind turbulence
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERSTELLAR PICKUP PROTONS; ALFVENIC TURBULENCE; ULYSSES OBSERVATIONS;
SPATIAL TRANSPORT; POLAR WIND; DISSIPATION; FLUCTUATIONS; PLASMA; 1-AU;
EVOLUTION
AB Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (1) the energy exchange timescale is very long and (2) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data.
C1 [Breech, B.] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20716 USA.
[Matthaeus, W. H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Cranmer, S. R.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Oughton, S.] Univ Waikato, Dept Math, Hamilton 3240, New Zealand.
RP Breech, B (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Mail Code 673,8800 Greenbelt Rd, Greenbelt, MD 20716 USA.
EM babreech@gmail.com
RI Kasper, Justin/D-1152-2010; Oughton, Sean/A-3380-2012
OI Kasper, Justin/0000-0002-7077-930X; Oughton, Sean/0000-0002-2814-7288
FU National Aeronautics and Space Administration (NASA) [NNG04GE77G,
NNX06AG95G, NNX09AB27G, NNX08AI47G, NNX08AW07G]; NSF [ATM 0752135]
FX Amitava Bhattacharjee thanks the reviewers for their assistance in
evaluating this paper.
NR 45
TC 45
Z9 45
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP 16
PY 2009
VL 114
AR A09103
DI 10.1029/2009JA014354
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 497KS
UT WOS:000270058700003
ER
PT J
AU MacPherson, GJ
Mittlefehldt, DW
Lipschutz, ME
Clayton, RN
Bullock, ES
Ivanov, AV
Mayeda, TK
Wang, MS
AF MacPherson, Glenn J.
Mittlefehldt, David W.
Lipschutz, Michael E.
Clayton, Robert N.
Bullock, Emma S.
Ivanov, Andrei V.
Mayeda, Toshiko K.
Wang, Ming-Sheng
TI The Kaidun chondrite breccia: Petrology, oxygen isotopes, and trace
element abundances
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CARBONACEOUS CHONDRITE; AQUEOUS ALTERATION; ENSTATITE CHONDRITE; MATRIX
MINERALOGY; CM CHONDRITES; TAGISH LAKE; METEORITE; CHONDRULES; CI;
GEOCHEMISTRY
AB Oxygen isotope and trace element data for 13 samples of the Kaidun chondritic breccia reaffirm the complex polymict nature of this unique meteorite. Bulk Kaidun samples most closely resemble CR chondrites, but the matrix is Cl-like. Two separated clasts are CR-like but have some properties that resemble CM, two clasts are enstatite chondrites (one EL and one EH), one clast is an aubrite-like metal-rich impact melt, and one clast is a unique layered olivine-bearing pyroxenite with the isotopic composition of an aubrite. Yet, although each clast resembles a known meteorite group, all deviate in some respect from the norms for those groups. Collectively, Kaidun has sampled materials not yet represented in the world meteorite collections and which greatly extend the definitions of known meteorite groups. Phyllosilicates in Kaidun span a very wide range in composition and vary from clast to clast, suggesting that the aqueous alteration experienced by the clasts predated assembly of the Kaidun parent body. Published by Elsevier Ltd.
C1 [MacPherson, Glenn J.; Bullock, Emma S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Lipschutz, Michael E.; Wang, Ming-Sheng] Purdue Univ, Dept Chem, BRWN WTHR, W Lafayette, IN 47907 USA.
[Clayton, Robert N.; Mayeda, Toshiko K.] Univ Chicago, Enciro Fermi Inst, Chicago, IL 60637 USA.
[Ivanov, Andrei V.] VI Vernadskii Inst Geochem & Analyt Chem, Moscow 119991, Russia.
RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
EM macphers@si.edu
FU NASA [NNG04GK47G, NNX07AJ05G, NAGW-3396]; NSF [9526747]; U.S. Department
of Energy [DE-FG07-011D1414]
FX Drs. Jcffrey Grossman, Herbert Palme, Ed Scott, and Michael Weisberg
provided detailed and very helpful reviews of the manuscript over
several versions, and we are indebted to them for their time and
patience. Dr. Jeffrey Post graciously helped with the X-ray diffraction
study of the metal phase in sample #01.3.01. This research was supported
by NASA Grants NNG04GK47G and NNX07AJ05G (GJM), NAGW-3396 (MEL), and NSF
Grant 9526747 (RNC). The NASA Cosmochemistry Program financed DWM's
participation. We thank the staff of the University of Missouri Research
Reactor for their aid and the U.S. Department of Energy for reactor
support under Grant DE-FG07-011D14146. We thank Mr. H. Mirzaci for
invaluable aid.
NR 46
TC 14
Z9 14
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 15
PY 2009
VL 73
IS 18
BP 5493
EP 5511
DI 10.1016/j.gca.2009.06.012
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 489EB
UT WOS:000269401600019
ER
PT J
AU Banks, ME
Lang, NP
Kargel, JS
McEwen, AS
Baker, VR
Grant, JA
Pelletier, JD
Strom, RG
AF Banks, Maria E.
Lang, Nicholas P.
Kargel, Jeffrey S.
McEwen, Alfred S.
Baker, Victor R.
Grant, John A.
Pelletier, Jon D.
Strom, Robert G.
TI An analysis of sinuous ridges in the southern Argyre Planitia, Mars
using HiRISE and CTX images and MOLA data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ESKER SYSTEM; ICE; GLACIATION; MELTWATER; SCALE; WATER; FLOW;
TOPOGRAPHY; MORPHOLOGY; EVOLUTION
AB A suite of sinuous ridges with branching and braided morphologies forms an anastomosing network in southern Argyre Planitia, Mars. Several modes of origin have been proposed for the Argyre ridges. Imagery from the High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX) aboard Mars Reconnaissance Orbiter (MRO) and Mars Orbiter Laser Altimeter (MOLA) topographic data sets from Mars Global Surveyor (MGS) are used to constrain processes involved in formation of the Argyre ridges. We find the characteristics of the ridges and associated layered deposits consistent with glaciofluvial-lacustrine processes and conclude that the ridges are most likely eskers. In particular, variations in ridge height appear to be related to the surrounding surface slope; ridge height increases with descending slopes and decreases with ascending slopes. This characteristic is observed in terrestrial eskers and is related to subice flow processes. The nature of some eroding beds in the ridges suggests induration. If the Argyre ridges are indeed eskers, the southern Argyre basin was once covered by the margin of a large, thick, stagnating or retreating ice deposit that extended for hundreds of kilometers or more. During ridge formation, water flowed on top, within, or beneath the ice deposit; the continuity and preservation of the ridges suggests that flow was primarily at the base of the ice. The dimensions (up to hundreds of meters tall and several kilometers wide), aspect ratio, and extent (hundreds of kilometers) of the ridges, as well as preliminary calculations of discharge, suggest that a significant amount of water was available.
C1 [Banks, Maria E.; Pelletier, Jon D.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Lang, Nicholas P.] Mercyhurst Coll, Dept Geol, Erie, PA 16546 USA.
[Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[McEwen, Alfred S.; Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
RP Banks, ME (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
FU NASA
FX We gratefully acknowledge the invaluable assistance of the entire HiRISE
team, including the software developers, the uplink and downlink teams,
and the science team. We would also like to thank H. J. Melosh, W. L.
Jaeger, S. Byrne, V. C. Gulick, R. M. E. Williams, N. Schofield, S.
Valesco, J. Wilfore, J. Sano, and C. M. Dundas for their comments,
suggestions, and encouragement and S. Mattson, who produced the DEM used
in this study. This paper also benefited from detailed reviews by J. W.
Head and an anonymous reviewer. This work was supported by the NASA Mars
Reconnaissance Orbiter project managed through the California Institute
of Technology's Jet Propulsion Laboratory.
NR 70
TC 25
Z9 26
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP 15
PY 2009
VL 114
AR E09003
DI 10.1029/2008JE003244
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 497KG
UT WOS:000270057500001
ER
PT J
AU De Grave, S
Pentcheff, ND
Ahyong, ST
Chan, TY
Crandall, KA
Dworschak, PC
Felder, DL
Feldmann, RM
Fransen, CHJM
Goulding, LYD
Lemaitre, R
Low, MEY
Martin, JW
Ng, PKL
Schweitzer, CE
Tan, SH
Tshudy, D
Wetzer, R
AF De Grave, Sammy
Pentcheff, N. Dean
Ahyong, Shane T.
Chan, Tin-Yam
Crandall, Keith A.
Dworschak, Peter C.
Felder, Darryl L.
Feldmann, Rodney M.
Fransen, Charles H. J. M.
Goulding, Laura Y. D.
Lemaitre, Rafael
Low, Martyn E. Y.
Martin, Joel W.
Ng, Peter K. L.
Schweitzer, Carrie E.
Tan, S. H.
Tshudy, Dale
Wetzer, Regina
TI A CLASSIFICATION OF LIVING AND FOSSIL GENERA OF DECAPOD CRUSTACEANS
SO RAFFLES BULLETIN OF ZOOLOGY
LA English
DT Review
DE Decapoda; Crustacea; Arthropoda; taxonomy; classification
ID FRESH-WATER CRAB; INDO-WEST PACIFIC; PONTONIINE SHRIMP CRUSTACEA; NOV
SP-NOV; N-SP CRUSTACEA; FAMILY PAGURIDAE CRUSTACEA; CRETACEOUS PIERRE
SHALE; INFAUNAL ALPHEID SHRIMP; PROTEIN-CODING GENES; COON CREEK
FORMATION
AB We present an updated classification for the entire Crustacea Decapoda, listing all known families and genera organized by higher taxonomic groups and including estimates of the number of species in every genus. All taxonomic names are also linked to the verified literature in which they were described, the first compilation of its kind for the Decapoda. To arrive at this compilation, we began with the classification scheme provided by Martin & Davis (2001) for extant families,, updated the higher classification and included the fossil taxa. The resultant framework was then populated with the currently valid genera and an estimate of species numbers within each genus. Our resulting classification, spanning both extant (living) and fossil taxa, is the first comprehensive estimate of taxonomic diversity within the entire Decapoda. The classification consists of 233 families of decapods containing 2,725 genera and an estimated 17,635 species (including both extant and fossil species). Of the families in our classification, 53 are exclusively fossil, 109 contain both fossil and extant species, and 71 are extant only. The current estimate for extant species is 14,756, whereas 2,979 species are known exclusively as fossils.
C1 [De Grave, Sammy; Goulding, Laura Y. D.] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England.
[Pentcheff, N. Dean; Martin, Joel W.; Wetzer, Regina] Nat Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA.
[Ahyong, Shane T.] NIWA, Marine Biodivers & Biosecur, Kilbirnie Wellington, New Zealand.
[Chan, Tin-Yam] Natl Taiwan Ocean Univ, Inst Marine Biol, Chilung 20224, Taiwan.
[Crandall, Keith A.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA.
[Crandall, Keith A.] Brigham Young Univ, Monte L Bean Life Sci Museum, Provo, UT 84602 USA.
[Dworschak, Peter C.] Nat Hist Museum, Dritte Zool Abt, Vienna, Austria.
[Felder, Darryl L.] Univ Louisiana, Dept Biol, Lafayette, LA 70504 USA.
[Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44242 USA.
[Fransen, Charles H. J. M.] Nat Hist Museum, NL-2300 RA Leiden, Netherlands.
[Lemaitre, Rafael] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Low, Martyn E. Y.; Ng, Peter K. L.; Tan, S. H.] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore.
[Schweitzer, Carrie E.] Kent State Univ, Dept Geol, N Canton, OH 44720 USA.
[Tshudy, Dale] Edinboro Univ Penn, Dept Geosci, Edinboro, PA 16444 USA.
RP De Grave, S (reprint author), Univ Oxford, Museum Nat Hist, Parks Rd, Oxford OX1 3PW, England.
EM sammy.degrave@oum.ox.ac.uk; pentcheff@gmail.com; s.ahyong@niwa.co.nz;
tychan@mail.ntou.edu.tw; keith.crandall@byu.edu;
Peter.Dworschak@nhm-wien.ac.at; dlf4517@louisiana.edu;
rfeldman@kent.edu; Fransen@naturalis.nnm.nl; lydgoulding@googlemail.com;
lemaitrr@si.edu; martyn@nus.edu.sg; jmartin@nhm.org; peterng@nus.edu.sg;
cschweit@kent.edu; sweehee@nus.edu.sg; dtshudy@edinboro.edu;
rwetzer@nhm.org
RI Low, Martyn/E-7525-2011; Ng, Peter/J-7393-2012; Fransen,
Charles/A-6693-2017
OI Fransen, Charles/0000-0002-7760-2603
NR 1320
TC 253
Z9 307
U1 5
U2 32
PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES
PI SINGAPORE
PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE
SN 0217-2445
J9 RAFFLES B ZOOL
JI Raffles Bull. Zool.
PD SEP 15
PY 2009
SU 21
BP 1
EP 109
PG 109
WC Zoology
SC Zoology
GA 504FR
UT WOS:000270601800001
ER
PT J
AU Xiang, F
Rudometkin, E
Churazov, E
Forman, W
Bohringer, H
AF Xiang, F.
Rudometkin, E.
Churazov, E.
Forman, W.
Boehringer, H.
TI Does heating by AGN shocks affect abundance profiles in galaxy clusters
?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: abundances; galaxies: clusters: general
ID ACTIVE GALACTIC NUCLEI; COOLING-CORE CLUSTERS; X-RAY EVIDENCE;
INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; GASEOUS ATMOSPHERE; BUOYANT
BUBBLES; XMM-NEWTON; M87; SOLAR
AB We evaluate the impact of gas shock heating by a central active galactic nuclei (AGN) in M87 on the radial distribution of heavy elements. The propagation of a shock creates an inverted entropy profile, and the subsequent rearrangement of the gaseous atmosphere transports metal-rich gas from the central region to larger radii. We show that for the parameters of the relatively weak shock, recently found in M87, the abundance profile is not strongly affected by the redistribution of the shock heated gas (except for the very central region). At the same time, the energetics of the source is fully sufficient to broaden the metal distribution to match the observations, strongly suggesting that mechanisms other than direct shock heating must operate in cluster cores. The absence of a very strong abundance peak at the very centre of M87 suggests that the central AGN produces frequent (every few 10 Myr) and relatively weak outbursts, rather than rarer (every few 100 Myr) and an order of magnitude more powerful events.
C1 [Xiang, F.; Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Rudometkin, E.; Churazov, E.] Space Res Inst IKI, Moscow 117997, Russia.
[Forman, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Boehringer, H.] MPI Extraterr Phys, D-85740 Garching, Germany.
RP Xiang, F (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
EM feiart66@gmail.com
RI Churazov, Eugene/A-7783-2013
FU DFG [CH389/3-2]; Russian Academy of Sciences
FX We are grateful to Hans-Thomas Janka for the provision of
one-dimensional Lagrangian hydrodynamics code, initially used for
supernovae explosion calculations. This work was supported by the DFG
grant CH389/3-2 and the program of the Russian Academy of Sciences
'Origin and evolution of stars and galaxies'.
NR 34
TC 2
Z9 2
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 11
PY 2009
VL 398
IS 2
BP 575
EP 582
DI 10.1111/j.1365-2966.2009.15139.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 490NH
UT WOS:000269507200007
ER
PT J
AU Shockley, FW
Vandenberg, NJ
AF Shockley, Floyd W.
Vandenberg, Natalia J.
TI Catalogue of the primary types of Cerylonidae, Endomychidae and
Latridiidae (Coleoptera: Cucujoidea) deposited in the National Museum of
Natural History, with additional notes and clarification of the status
of several types
SO ZOOTAXA
LA English
DT Article
DE Cerylonidae; Endomychidae; Latridiidae; USNM types; catalogue
AB A checklist with critical data is provided for all primary types (n = 48) of the families Cerylonidae, Endomychidae and Latridiidae deposited in the National Museum of Natural History. Of those, 43 holotypes, 3 lectotypes, and 2 neotypes are represented. This tally includes a lectotype for Geoendomychus punctatus Arrow (1926) and neotype for Rhymbomicrus stephani Pakaluk (1987), both newly designated to promote nomenclatural stability. Fifteen species have at least one paratype, paralectotype, or authoritatively identified non-type specimen associated with the holotype. Type specimens were compared to the original species descriptions to confirm their status, verbatim label data were recorded, and barcode labels were added. In addition to cataloguing the types, notes were made where discrepancies exist between the data labels pinned with the types and the data published with the original species descriptions.
C1 [Shockley, Floyd W.] Univ Georgia, Dept Entomol, Athens, GA 30602 USA.
[Vandenberg, Natalia J.] ARS, SEL, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Shockley, FW (reprint author), Univ Georgia, Dept Entomol, 413 Biol Sci Bldg, Athens, GA 30602 USA.
EM fws@uga.edu; Natalia.Vandenberg@ars.usda.gov
FU Smithsonian Institution [0000132599]; H. H. Ross Fund (Dept. of
Entomology, University of Georgia) and through an NSF/PEET [DEB-0329115]
FX We thank S. McKamey (SEL), A. Norrbom (SEL) and J. McHugh (University of
Georgia) and two anonymous reviewers for reviewing earlier drafts of
this manuscript and providing many helpful suggestions. We gratefully
acknowledge L. Roberts and M. Metz (SEL) for assistance with type
imaging, and W. Steiner for information on and access to the Casey
collection. We thank E. Riley (Texas A&M University) for confirming the
number and identity of the R. stephani paratypes housed in the Stephan
collection and P. Skelley (Florida State Collection of Arthropods) for
confirming that the missing holotype of R. stephani was not deposited at
the FSCA. We also thank S. Lingafelter for loaning his Canon EOS digital
camera which was used to photograph the type labels. We acknowledge T.
Orrell and M. Vanzego for their assistance with setting up the logistics
and paperwork for the contract under which this work was accomplished.
We further thank R. Snyder for making the electronic products of this
contract (including dorsal, ventral and lateral habitus images and the
specimen data labels) accessible via the Smithsonian KE EMu system. Most
of this work was internally funded by the Smithsonian Institution
through Contract No.: 0000132599. The remainder of the work was funded
jointly by the H. H. Ross Fund (Dept. of Entomology, University of
Georgia) and through an NSF/PEET grant (DEB-0329115) to J. McHugh, M.
Whiting and K. Miller.
NR 29
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 SEP 11
PY 2009
IS 2229
BP 1
EP 64
PG 64
WC Zoology
SC Zoology
GA 492XY
UT WOS:000269697200001
ER
PT J
AU Devereux, N
Willner, SP
Ashby, MLN
Willmer, CNA
Hriljac, P
AF Devereux, Nick
Willner, S. P.
Ashby, M. L. N.
Willmer, C. N. A.
Hriljac, Paul
TI NEARBY GALAXIES IN THE 2 mu m ALL SKY SURVEY. I. K-BAND LUMINOSITY
FUNCTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: bulges; galaxies: elliptical and lenticular, cD; galaxies:
formation; galaxies: luminosity function, mass function; galaxies:
spiral; infrared: galaxies
ID SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; REDSHIFT SURVEY;
ELLIPTIC GALAXIES; COSMOLOGICAL FRAMEWORK; CLUSTER GALAXIES; SPACE
DENSITY; MASS FUNCTION; RED GALAXIES; EVOLUTION
AB Differential K-s-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall K-s-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the K-s-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at K-s in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.
C1 [Devereux, Nick] Embry Riddle Aeronaut Univ, Dept Phys, Prescott, AZ 86301 USA.
[Willner, S. P.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Willmer, C. N. A.] Univ Arizona, Tucson, AZ 85721 USA.
[Hriljac, Paul] Embry Riddle Aeronaut Univ, Dept Math & Comp Sci, Prescott, AZ 86301 USA.
RP Devereux, N (reprint author), Natl Univ Ireland, Ctr Astron, Galway, Ireland.
EM devereux@erau.edu; swillner@cfa.harvard.edu; mashby@cfa.harvard.edu;
cnaw@as.arizona.edu; hriljap@erau.edu
FU Fulbright Commission; National University of Ireland, Galway; National
Aeronautics and Space Administration; National Science Foundation
FX N. D. gratefully acknowledges the support of the Fulbright Commission
and the hospitality of the National University of Ireland, Galway, and
the assistance of undergraduate students Meghan Burleigh, Sarah
McNamara, and Lisa Fallon for their help in the early stages of this
project. Extensive use was made of the HyperLeda database
(http://leda.univ-lyon1.fr) and data products from the Two Micron All
Sky Survey, which is a joint project of the University of Massachusetts
and the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. The Millennium Simulation databases
used in this paper and the Web application providing online access to
them were constructed as part of the activities of the German
Astrophysical Virtual Observatory. We thank Darren Croton and Gerard
Lemson for help with the database tools. We thank Daniel Eisenstein for
supplying the galaxy correlation function used in the cosmic variance
calculation. We thank John Huchra for providing galaxy redshifts in
advance of publication and Alessandro Marconi and Francesco Shankar for
digitized BHMFs.
NR 91
TC 14
Z9 14
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2009
VL 702
IS 2
BP 955
EP 969
DI 10.1088/0004-637X/702/2/955
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BI
UT WOS:000269245000014
ER
PT J
AU Lee, JC
Xiang, JG
Ravel, B
Kortright, J
Flanagan, K
AF Lee, Julia C.
Xiang, Jingen
Ravel, Bruce
Kortright, Jeffrey
Flanagan, Kathryn
TI CONDENSED MATTER ASTROPHYSICS: A PRESCRIPTION FOR DETERMINING THE
SPECIES-SPECIFIC COMPOSITION AND QUANTITY OF INTERSTELLAR DUST USING
X-RAYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances; dust, extinction; ISM: molecules; methods: data
analysis; methods: laboratory; techniques: spectroscopic; X-rays: ISM
ID ABSORPTION FINE-STRUCTURE; PERTURBATION-THEORY APPROACH; IRON;
SPECTROSCOPY; FE; TRANSMISSION; WAVELENGTHS; REFLECTION; SCATTERING;
SPECTRUM
AB We present a new technique for determining the quantity and composition of dust in astrophysical environments using <6 keV X-rays. We argue that high-resolution X-ray spectra as enabled by the Chandra and XMM-Newton gratings should be considered a powerful and viable new resource for delving into a relatively unexplored regime for directly determining dust properties: composition, quantity, and distribution. We present initial cross section measurements of astrophysically likely iron-based dust candidates taken at the Lawrence Berkeley National Laboratory Advanced Light Source synchrotron beamline, as an illustrative tool for the formulation of our technique for determining the quantity and composition of interstellar dust with X-rays. (Cross sections for the materials presented here will be made available for astrophysical modeling in the near future.) Focused at the 700 eV Fe L-III and L-II photoelectric edges, we discuss a technique for modeling dust properties in the soft X-rays using L-edge data to complement K-edge X-ray absorption fine structure analysis techniques discussed by Lee & Ravel. The paper is intended to be a techniques paper of interest and useful to both condensed matter experimentalists and astrophysicists. For the experimentalists, we offer a new prescription for normalizing relatively low signal-to-noise ratio L-edge cross section measurements. For astrophysics interests, we discuss the use of X-ray absorption spectra for determining dust composition in cold and ionized astrophysical environments and a new method for determining species-specific gas and dust ratios. Possible astrophysical applications of interest, including relevance to Sagittarius A*, are offered. Prospects for improving on this work in future X-ray missions with higher throughput and spectral resolution are also presented in the context of spectral resolution goals for gratings and calorimeters, for proposed and planned missions such as Astro-H and the International X-ray Observatory.
C1 [Lee, Julia C.; Xiang, Jingen] Harvard Univ, Dept Astron, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ravel, Bruce] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
[Kortright, Jeffrey] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Mat Sci, Berkeley, CA 94720 USA.
[Flanagan, Kathryn] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Lee, JC (reprint author), Harvard Univ, Dept Astron, Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 6, Cambridge, MA 02138 USA.
RI MSD, Nanomag/F-6438-2012; Lee, Julia/G-2381-2015
OI Lee, Julia/0000-0002-7336-3588
FU U.S. Department of Energy [DE-AC02-05CH11231]; Harvard Faculty of Arts
and Sciences; [SAO AR8-9007]
FX We acknowledge Eric Gullickson, Pannu Nachimuthu, and Elke Arenholz for
beamline support. We thank Claude Canizares and Alex Dalgarno for advice
and conversations, and Fred Baganoff for discussions relating to Sgr A*.
The Advanced Light Source and JKB 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. J. C. L. is grateful to
Chandra grant SAO AR8-9007 and the Harvard Faculty of Arts and Sciences
for financial support.
NR 28
TC 23
Z9 23
U1 0
U2 6
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 SEP 10
PY 2009
VL 702
IS 2
BP 970
EP 979
DI 10.1088/0004-637X/702/2/970
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BI
UT WOS:000269245000015
ER
PT J
AU Simon, JD
Gal-Yam, A
Gnat, O
Quimby, RM
Ganeshalingam, M
Silverman, JM
Blondin, S
Li, WD
Filippenko, AV
Wheeler, JC
Kirshner, RP
Patat, F
Nugent, P
Foley, RJ
Vogt, SS
Butler, RP
Peek, KMG
Rosolowsky, E
Herczeg, GJ
Sauer, DN
Mazzali, PA
AF Simon, Joshua D.
Gal-Yam, Avishay
Gnat, Orly
Quimby, Robert M.
Ganeshalingam, Mohan
Silverman, Jeffrey M.
Blondin, Stephane
Li, Weidong
Filippenko, Alexei V.
Wheeler, J. Craig
Kirshner, Robert P.
Patat, Ferdinando
Nugent, Peter
Foley, Ryan J.
Vogt, Steven S.
Butler, R. Paul
Peek, Kathryn M. G.
Rosolowsky, Erik
Herczeg, Gregory J.
Sauer, Daniel N.
Mazzali, Paolo A.
TI VARIABLE SODIUM ABSORPTION IN A LOW-EXTINCTION TYPE Ia SUPERNOVA
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE circumstellar matter; supernovae: general; supernovae: individual (SN
1999cl, SN 2006X, SN 2007le)
ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; HIGH-VELOCITY FEATURES; BRAHES 1572
SUPERNOVA; STANDARD TYPE IA; DARK ENERGY; SECONDARY STAR; LIGHT-ECHO;
CIRCUMSTELLAR INTERACTION; INTERSTELLAR ABSORPTION; SPECTRUM SYNTHESIS
AB Recent observations have revealed that some Type Ia supernovae exhibit narrow, time-variable Na I D absorption features. The origin of the absorbing material is controversial, but it may suggest the presence of circumstellar gas in the progenitor system prior to the explosion, with significant implications for the nature of the supernova (SN) progenitors. We present the third detection of such variable absorption, based on six epochs of high-resolution spectroscopy of the Type Ia supernova SN 2007le from the Keck I Telescope and the Hobby - Eberly Telescope. The data span a time frame of approximately three months, from 5 days before maximum light to 90 days after maximum. We find that one component of the Na I D absorption lines strengthened significantly with time, indicating a total column density increase of similar to 2.5 x 10(12) cm(-2). The data limit the typical timescale for the variability to be more than 2 days but less than 10 days. The changes appear to be most prominent after maximum light rather than at earlier times when the ultraviolet flux from the SN peaks. As with SN 2006X, we detect no change in the Ca II H and K absorption lines over the same time period, rendering line-of-sight effects improbable and suggesting a circumstellar origin for the absorbing material. Unlike the previous two supernovae exhibiting variable absorption, SN 2007le is not highly reddened (EB-V = 0.27 mag), also pointing toward circumstellar rather than interstellar absorption. Photoionization calculations show that the data are consistent with a dense (10(7) cm(-3)) cloud or clouds of gas located similar to 0.1 pc (3 x 10(17) cm) from the explosion. These results broadly support the single-degenerate scenario previously proposed to explain the variable absorption, with mass loss from a nondegenerate companion star responsible for providing the circumstellar gas. We also present possible evidence for narrow Ha emission associated with the SN, which will require deep imaging and spectroscopy at late times to confirm.
C1 [Simon, Joshua D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Quimby, Robert M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Ganeshalingam, Mohan; Silverman, Jeffrey M.; Li, Weidong; Filippenko, Alexei V.; Peek, Kathryn M. G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Blondin, Stephane; Patat, Ferdinando] European So Observ, D-85748 Garching, Germany.
[Wheeler, J. Craig] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Kirshner, Robert P.; Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nugent, Peter] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Vogt, Steven S.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Butler, R. Paul] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Rosolowsky, Erik] Univ British Columbia, Dept Phys, Okanagan, BC V1V 1V7, Canada.
[Herczeg, Gregory J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Sauer, Daniel N.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Mazzali, Paolo A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Mazzali, Paolo A.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Mazzali, Paolo A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
RP Simon, JD (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM jsimon@ociw.edu; avishay.gal-yam@weizmann.ac.il;
orlyg@tapir.caltech.edu; quimby@astro.caltech.edu;
mganesh@astro.berkeley.edu; jsilverman@astro.berkeley.edu;
sblondin@eso.org; weidong@astro.berkeley.edu; alex@astro.berkeley.edu;
wheel@astro.as.utexas.edu; kirshner@cfa.harvard.edu; fpatat@eso.org;
penugent@lbl.gov; rfoley@cfa.harvard.edu; vogt@ucolick.org;
butler@dtm.ciw.edu; kpeek@astro.berkeley.edu; erik.rosolowsky@ubc.ca;
gregoryh@mpe.mpg.de; dsauer@astro.su.se; mazzali@mpa-garching.mpg.de
RI Butler, Robert/B-1125-2009; Sauer, Daniel/A-3033-2012;
OI Sauer, Daniel/0000-0002-0317-5063; Patat,
Ferdinando/0000-0002-0537-3573; Herczeg, Gregory/0000-0002-7154-6065
FU Carnegie Institution of Washington; Israeli Science Foundation; EU
Seventh Framework Programme Marie Curie IRG fellowship; Ministry of
Science, Culture Sport, Israel; Ministry of Research, France; NSF
[AST-0707769, AST-0607485, AST 0606772]; US Department of Energy
[DE-FG02-08ER41563]; TABASGO Foundation; Sun Microsystems, Inc;
Hewlett-Packard Company
FX J. D. S. acknowledges the support of a Millikan Fellowship provided by
Caltech and a Vera Rubin Fellowship from the Carnegie Institution of
Washington. A. G. acknowledges support by the Israeli Science
Foundation; an EU Seventh Framework Programme Marie Curie IRG
fellowship; the Ministry of Science, Culture & Sport, Israel and the
Ministry of Research, France; and the Benoziyo Center for Astrophysics,
UK-Weizmann fund, a research grant from the Peter and Patricia Gruber
Awards, and the William Z. and Eda Bess Novick New Scientists Fund at
the Weizmann Institute. R. Q. and J. C. W. are supported in part by NSF
grant AST-0707769. A. V. F.'s supernova group at U. C. Berkeley is
supported by NSF grant AST-0607485, US Department of Energy grant
DE-FG02-08ER41563, and the TABASGO Foundation. KAIT and its ongoing
operation were made possible by donations from Sun Microsystems, Inc.,
the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory,
the NSF, the University of California, the Sylvia & Jim Katzman
Foundation, and the TABASGO Foundation. Supernova research at the
Harvard College Observatory is supported in part by the NSF through AST
0606772.
NR 106
TC 106
Z9 106
U1 0
U2 6
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 SEP 10
PY 2009
VL 702
IS 2
BP 1157
EP 1170
DI 10.1088/0004-637X/702/2/1157
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BI
UT WOS:000269245000031
ER
PT J
AU Attard, M
Houde, M
Novak, G
Li, HB
Vaillancourt, JE
Dowell, CD
Davidson, J
Shinnaga, H
AF Attard, Michael
Houde, Martin
Novak, Giles
Li, Hua-bai
Vaillancourt, John E.
Dowell, C. Darren
Davidson, Jacqueline
Shinnaga, Hiroko
TI MAGNETIC FIELDS AND INFALL MOTIONS IN NGC 1333 IRAS 4
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual (NGC 1333 IRAS 4); ISM: magnetic fields; ISM: molecules;
polarization; stars: formation; submillimeter
ID POLARIZED DUST EMISSION; MOLECULAR CLOUD CORES; STAR-FORMATION; NGC-1333
IRAS-4; INTERSTELLAR CLOUDS; PROFILES; COLLAPSE; OUTFLOW; MODELS; LINE
AB We present single-dish 350 mu m dust continuum polarimetry as well as HCN and HCO+ J = 4 -> 3 rotational emission spectra obtained on NGC 1333 IRAS 4. The polarimetry indicates a uniform field morphology over a 20 '' radius from the peak continuum flux of IRAS 4A, in agreement with models of magnetically supported cloud collapse. The field morphology around IRAS 4B appears to be quite distinct, however, with indications of depolarization observed toward the peak flux of this source. Inverse P Cygni profiles are observed in the HCN J = 4 -> 3 line spectra toward IRAS 4A, providing a clear indication of infall gas motions. Taken together, the evidence gathered here appears to support the scenario that IRAS 4A is a cloud core in a critical state of support against gravitational collapse.
C1 [Attard, Michael; Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Li, Hua-bai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vaillancourt, John E.; Dowell, C. Darren] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Dowell, C. Darren] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davidson, Jacqueline] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia.
[Shinnaga, Hiroko] CALTECH, Submillimeter Observ, Hilo, HI 96720 USA.
RP Attard, M (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
EM mattard@uwo.ca
FU NSERC; Canada Foundation for Innovation; Ontario Innovation Trust;
Western's Academic Development Fund; NSF [AST 05-40882, AST 02-43156,
AST 05-05230, AST 05-05124]
FX Our group is grateful for the assistance of the Caltech Sub-millimeter
Observatory staff in installing and observing with SHARP and the
heterodyne receiver. We also acknowledge the help provided by Jose
Girart, Megan Krejny, Roger Hildebrand, Tristan Matthews, Larry Kirby,
and Lerothodi Leeuw. M. A.' s and M.H.'s research is funded through the
NSERC Discovery Grant, Canada Research Chair, Canada Foundation for
Innovation, Ontario Innovation Trust, and Western's Academic Development
Fund programs. SHARC II is funded through the NSF grant AST 05-40882 to
the California Institute of Technology. The development of SHARP was
funded by an NSF grant to Northwestern University (AST 02-43156), and
its subsequent commissioning was funded by NSF grants to Northwestern
University (AST 05-05230) and University of Chicago (AST 05-05124).
NR 35
TC 22
Z9 22
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2009
VL 702
IS 2
BP 1584
EP 1592
DI 10.1088/0004-637X/702/2/1584
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BI
UT WOS:000269245000064
ER
PT J
AU Cranmer, SR
Matthaeus, WH
Breech, BA
Kasper, JC
AF Cranmer, Steven R.
Matthaeus, William H.
Breech, Benjamin A.
Kasper, Justin C.
TI EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR
WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE hydrodynamics; MHD; plasmas; solar wind; turbulence; waves
ID ANISOTROPIC MAGNETOHYDRODYNAMIC TURBULENCE; 1 AU; ALFVENIC TURBULENCE;
LOW-FREQUENCY; HYDROMAGNETIC TURBULENCE; VELOCITY DISTRIBUTIONS; ULYSSES
OBSERVATIONS; INTERSTELLAR-MEDIUM; ACCRETION FLOWS; MHD TURBULENCE
AB We analyze measured proton and electron temperatures in the high-speed solar wind in order to calculate the separate rates of heat deposition for protons and electrons. When comparing with other regions of the heliosphere, the fast solar wind has the lowest density and the least frequent Coulomb collisions. This makes the fast wind an optimal testing ground for studies of collisionless kinetic processes associated with the dissipation of plasma turbulence. Data from the Helios and Ulysses plasma instruments were collected to determine mean radial trends in the temperatures and the electron heat conduction flux between 0.29 and 5.4 AU. The derived heating rates apply specifically for these mean plasma properties and not for the full range of measured values around the mean. We found that the protons receive about 60% of the total plasma heating in the inner heliosphere, and that this fraction increases to approximately 80% by the orbit of Jupiter. A major factor affecting the uncertainty in this fraction is the uncertainty in the measured radial gradient of the electron heat conduction flux. The empirically derived partitioning of heat between protons and electrons is in rough agreement with theoretical predictions from a model of linear Vlasov wave damping. For a modeled power spectrum consisting only of Alfvenic fluctuations, the best agreement was found for a distribution of wavenumber vectors that evolves toward isotropy as distance increases.
C1 [Cranmer, Steven R.; Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA.
[Breech, Benjamin A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM scranmer@cfa.harvard.edu
RI Kasper, Justin/D-1152-2010
OI Kasper, Justin/0000-0002-7077-930X
FU National Aeronautics and Space Administration (NASA) [NNG04GE77G,
NNX06AG95G, NNX09AB27G, NNX08AI47G, NNX08AW07G]; NSF [ATM 0752135]
FX The authors thank Adriaan van Ballegooijen and Eliot Quataert for
valuable discussions. S.R.C.'s work was supported by the National
Aeronautics and Space Administration (NASA) under grants NNG04GE77G,
NNX06AG95G, and NNX09AB27G to the Smithsonian Astrophysical Observatory.
W.H.M.'s research was supported by NSF ATM 0752135 (SHINE) and NASA
NNX08AI47G (Heliophysics Theory Program). B.A.B.'s research was
supported in part by an appointment to the NASA Postdoctoral Program at
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. J.C.K.'s research was
supported in part by NASA grant NNX08AW07G.
NR 117
TC 76
Z9 76
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 SEP 10
PY 2009
VL 702
IS 2
BP 1604
EP 1614
DI 10.1088/0004-637X/702/2/1604
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BI
UT WOS:000269245000066
ER
PT J
AU An, D
Ramirez, SV
Sellgren, K
Arendt, RG
Boogert, ACA
Schultheis, M
Stolovy, SR
Cotera, AS
Robitaille, TP
Smith, HA
AF An, Deokkeun
Ramirez, Solange V.
Sellgren, Kris
Arendt, Richard G.
Boogert, A. C. Adwin
Schultheis, Mathias
Stolovy, Susan R.
Cotera, Angela S.
Robitaille, Thomas P.
Smith, Howard A.
TI FIRST SPECTROSCOPIC IDENTIFICATION OF MASSIVE YOUNG STELLAR OBJECTS IN
THE GALACTIC CENTER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE infrared: ISM; ISM: molecules; stars: formation
ID SPITZER-SPACE-TELESCOPE; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL
ENERGY-DISTRIBUTIONS; INFRARED ARRAY CAMERA; CARBON-DIOXIDE; MU-M;
PROTOSTELLAR ENVELOPES; MOLECULAR CLOUDS; ISO-SWS; STARS
AB We report the detection of several molecular gas-phase and ice absorption features in three photometrically selected young stellar object (YSO) candidates in the central 280 pc of the Milky Way. Our spectra, obtained with the Infrared Spectrograph (IRS) onboard the Spitzer Space Telescope, reveal gas-phase absorption from CO2 (15.0 mu m), C2H2 (13.7 mu m), and HCN (14.0 mu m). We attribute this absorption to warm, dense gas in massive YSOs. We also detect strong and broad 15 mu m CO2 ice absorption features, with a remarkable double-peaked structure. The prominent long-wavelength peak is due to CH3OH-rich ice grains, and is similar to those found in other known massive YSOs. Our IRS observations demonstrate the youth of these objects, and provide the first spectroscopic identification of massive YSOs in the Galactic Center.
C1 [An, Deokkeun; Boogert, A. C. Adwin] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Ramirez, Solange V.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Arendt, Richard G.] NASA, CREST, UMBC, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schultheis, Mathias] Observ Besancon, F-25000 Besancon, France.
[Schultheis, Mathias] CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Stolovy, Susan R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Cotera, Angela S.] SETI Inst, Mountain View, CA 94043 USA.
[Robitaille, Thomas P.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP An, D (reprint author), CALTECH, Ctr Infrared Proc & Anal, Mail Stop 100-22, Pasadena, CA 91125 USA.
EM deokkeun@ipac.caltech.edu; sellgren@astronomy.ohio-state.edu
OI Arendt, Richard/0000-0001-8403-8548; Robitaille,
Thomas/0000-0002-8642-1329
FU NASA through an award issued by JPL/Caltech
FX Support for this work was provided by NASA through an award issued by
JPL/Caltech. This research has made use of the SIMBAD database, operated
at CDS, Strasbourg, France.
NR 47
TC 8
Z9 8
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 SEP 10
PY 2009
VL 702
IS 2
BP L128
EP L132
DI 10.1088/0004-637X/702/2/L128
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BN
UT WOS:000269245500007
ER
PT J
AU Birnboim, Y
AF Birnboim, Yuval
TI MAGNETICALLY REGULATED GAS ACCRETION IN HIGH-REDSHIFT GALACTIC DISKS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: high-redshift; galaxies: ISM; galaxies: magnetic fields
ID ULTRA DEEP FIELD; GALAXY FORMATION; STAR-FORMATION; HYDROSTATIC
EQUILIBRIUM; DYNAMICAL EVOLUTION; INTERSTELLAR-MEDIUM; CLUMPY GALAXIES;
RAPID FORMATION; COLD FLOWS; MORPHOLOGIES
AB Disk galaxies are in hydrostatic equilibrium along their vertical axis. The pressure allowing for this configuration consists of thermal, turbulent, magnetic, and cosmic-ray components. For the Milky Way the thermal pressure contributes similar to 10% of the total pressure near the plane, with this fraction dropping toward higher altitudes. Out of the rest, magnetic fields contribute similar to 1/3 of the pressure to distances of similar to 3 kpc above the disk plane. In this Letter, we attempt to extrapolate these local values to high-redshift, rapidly accreting, rapidly star-forming disk galaxies and study the effect of the extra pressure sources on the accretion of gas onto the galaxies. In particular, magnetic field tension may convert a smooth cold-flow accretion to clumpy, irregular star formation regions and rates. The infalling gas accumulates on the edge of the magnetic fields, supported by magnetic tension. When the mass of the infalling gas exceeds some threshold mass, its gravitational force cannot be balanced by magnetic tension anymore, and it falls toward the disk's plane, rapidly making stars. Simplified estimations of this threshold mass are consistent with clumpy star formation observed in SINS, UDF, GOODS, and GEMS surveys. We discuss the shortcomings of pure hydrodynamic codes in simulating the accretion of cold flows into galaxies, and emphasize the need for magnetohydrodynamic simulations.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Birnboim, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Birnboim, Yuval/0000-0002-6547-8545
NR 33
TC 3
Z9 3
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2009
VL 702
IS 2
BP L101
EP L104
DI 10.1088/0004-637X/702/2/L101
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BN
UT WOS:000269245500001
ER
PT J
AU Fragos, T
Kalogera, V
Willems, B
Belczynski, K
Fabbiano, G
Brassington, NJ
Kim, DW
Angelini, L
Davies, RL
Gallagher, JS
King, AR
Pellegrini, S
Trinchieri, G
Zepf, SE
Zezas, A
AF Fragos, T.
Kalogera, V.
Willems, B.
Belczynski, K.
Fabbiano, G.
Brassington, N. J.
Kim, D. -W.
Angelini, L.
Davies, R. L.
Gallagher, J. S.
King, A. R.
Pellegrini, S.
Trinchieri, G.
Zepf, S. E.
Zezas, A.
TI TRANSIENT LOW-MASS X-RAY BINARY POPULATIONS IN ELLIPTICAL GALAXIES NGC
3379 AND NGC 4278
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: close; galaxies: elliptical and lenticular, cD; stars:
evolution; X-rays: binaries
ID CHANDRA MONITORING OBSERVATIONS; ULTRACOMPACT BINARIES; LUMINOSITY
FUNCTION; GLOBULAR-CLUSTERS; IRRADIATION; INSTABILITY; EVOLUTION;
CATALOG; STARS
AB We propose a physically motivated and self-consistent prescription for the modeling of transient neutron star low-mass X-ray binary (LMXB) properties, such as duty cycle (DC), outburst duration, and recurrence time. We apply this prescription to the population synthesis models of field LMXBs presented by Fragos et al., and compare the transient LMXB population to the Chandra X-ray survey of the two elliptical galaxies NGC 3379 and NGC 4278, which revealed several transient sources. We are able to exclude models with a constant DC for all transient systems, while models with a variable DC based on the properties of each system are consistent with the observed transient populations. We predict that the majority of the observed transient sources in these two galaxies are LMXBs with red giant donors. Finally, our comparison suggests that transient LMXBs are very rare in globular clusters (GCs), and thus the number of identified transient LMXBs may be used as a tracer of the relative contribution of field and GC LMXB populations.
C1 [Fragos, T.; Kalogera, V.; Willems, B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Belczynski, K.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Fabbiano, G.; Brassington, N. J.; Kim, D. -W.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Angelini, L.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Davies, R. L.] Univ Oxford, Oxford OX1 3RH, England.
[Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[King, A. R.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Trinchieri, G.] Observ Astron Brera, INAF, I-20121 Milan, Italy.
[Zepf, S. E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
RP Fragos, T (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA.
EM tassosfragos@northwestern.edu; vicky@northwestern.edu;
kbelczyn@nmsu.edu; gfabbiano@cfa.harvard.edu;
nbrassington@head.cfa.harvard.edu; kim@cfa.harvard.edu;
angelini@davide.gsfc.nasa.gov; rld@astro.ox.ac.uk; jsg@astro.wisc.edu;
ark@star.le.ac.uk; silvia.pellegrini@unibo.it;
ginevra.trinchieri@brera.inaf.it; zepf@pa.msu.edu;
azezas@cfa.harvard.edu
RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016
OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri,
Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523
FU Northwestern Presidential Fellowship
FX T.F. acknowledges support from the Northwestern Presidential Fellowship.
NR 23
TC 16
Z9 16
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2009
VL 702
IS 2
BP L143
EP L147
DI 10.1088/0004-637X/702/2/L143
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BN
UT WOS:000269245500010
ER
PT J
AU Halfen, DT
Ziurys, LM
Brunken, S
Gottlieb, CA
McCarthy, MC
Thaddeus, P
AF Halfen, D. T.
Ziurys, L. M.
Bruenken, S.
Gottlieb, C. A.
McCarthy, M. C.
Thaddeus, P.
TI DETECTION OF A NEW INTERSTELLAR MOLECULE: THIOCYANIC ACID HSCN
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual (Sgr B2); ISM: molecules; line: identification;
molecular processes; radio lines: ISM
ID ISOTHIOCYANIC ACID; SAGITTARIUS B2; ISOMERS; SPECTRA; REGION; HNCS
AB A new interstellar molecule, HSCN (thiocyanic acid), an energetic isomer of the well-known species HNCS, has been detected toward Sgr B2(N) with the Arizona Radio Observatory 12 m telescope. Eight rotational transitions in the K(a) = 0 ladder were observed in the 2 mm and 3 mm bands. Five consecutive transitions in the 3 mm band are unblended, but three in the 2 mm band are partially masked by lines of other molecules. The peak intensity of all eight transitions are well described by a rotational temperature that is in very good agreement with that of many other molecules in this source. The line width and radial velocity of HSCN match closely with those of the ground state isomer HNCS (isothiocyanic acid), HNCO (isocyanic acid), and HOCN (cyanic acid); preliminary maps indicate that all four molecules are similarly distributed in Sgr B2. Although HSCN is calculated to lie over 3000 K higher in energy than HNCS, its column density of 1.3 x 10(13) cm(-2) in Sgr B2(N) is only three times lower than that of HNCS. The fractional abundances of HSCN and HNCS relative to H(2) are 4.5 x 10(-12) and 1.1 x 10(-11). By analogy with the isomeric pair HCN and HNC, these two sulfur-bearing isomers are plausibly formed from a common cation precursor.
C1 [Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Dept Chem, Arizona Radio Observ, Tucson, AZ 85721 USA.
[Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Dept Astron, Arizona Radio Observ, Tucson, AZ 85721 USA.
[Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bruenken, S.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bruenken, S.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
RP Halfen, DT (reprint author), Univ Arizona, Dept Chem, Arizona Radio Observ, Tucson, AZ 85721 USA.
EM halfendt@as.arizona.edu; lziurys@as.arizona.edu;
sbruenken@cfa.harvard.edu; cgottlieb@cfa.harvard.edu;
mccarthy@cfa.harvard.edu; pthaddeus@cfa.harvard.edu
RI Brunken, Sandra/B-1880-2010;
OI Brunken, Sandra/0000-0001-7175-4828; McCarthy,
Michael/0000-0001-9142-0008; Halfen, DeWayne/0000-0003-2483-3616
FU National Science Foundation (NSF) [CHE 08-47919]; NSF Astronomy and
Astrophysics Postdoctoral Fellowship [AST 06-02282]
FX We thank the staff of ARO for supporting these observations, and A. J.
Remijan for communicating work in progress. The work here was supported
in part by the National Science Foundation (NSF) Center for Chemical
Innovation (CCI) grant CHE 08-47919. D. T. H. is supported by an NSF
Astronomy and Astrophysics Postdoctoral Fellowship under award AST
06-02282.
NR 17
TC 30
Z9 30
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2009
VL 702
IS 2
BP L124
EP L127
DI 10.1088/0004-637X/702/2/L124
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BN
UT WOS:000269245500006
ER
PT J
AU Hui, YW
Schultz, DR
Kharchenko, VA
Stancil, PC
Cravens, TE
Lisse, CM
Dalgarno, A
AF Hui, Yawei
Schultz, David R.
Kharchenko, Vasili A.
Stancil, Phillip C.
Cravens, Thomas E.
Lisse, Carey M.
Dalgarno, Alexander
TI THE ION-INDUCED CHARGE-EXCHANGE X-RAY EMISSION OF THE JOVIAN AURORAS:
MAGNETOSPHERIC OR SOLAR WIND ORIGIN?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE atomic processes; planets and satellites: individual (Jupiter)
ID XMM-NEWTON; CHANDRA OBSERVATIONS; JUPITER; OXYGEN; PRECIPITATION;
SPECTRA; TRANSITIONS; ATMOSPHERE; SCATTERING; PLANETS
AB A new and more comprehensive model of charge-exchange induced X-ray emission, due to ions precipitating into the Jovian atmosphere near the poles, has been used to analyze spectral observations made by the Chandra X-ray Observatory. The model includes for the first time carbon ions, in addition to the oxygen and sulfur ions previously considered, in order to account for possible ion origins from both the solar wind and the Jovian magnetosphere. By comparing the model spectra with newly reprocessed Chandra observations, we conclude that carbon ion emission provides a negligible contribution, suggesting that solar wind ions are not responsible for the observed polar X-rays. In addition, results of the model fits to observations support the previously estimated seeding kinetic energies of the precipitating ions (similar to 0.7-2 MeV u(-1)), but infer a different relative sulfur-to-oxygen abundance ratio for these Chandra observations.
C1 [Hui, Yawei; Schultz, David R.] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA.
[Kharchenko, Vasili A.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Stancil, Phillip C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Stancil, Phillip C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA.
[Cravens, Thomas E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, SD SRE, Laurel, MD 20723 USA.
[Dalgarno, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hui, YW (reprint author), Oak Ridge Natl Lab, Div Phys, Bldg 6010, Oak Ridge, TN 37831 USA.
EM huiy@ornl.gov; schultzd@ornl.gov; kharchenko@phys.uconn.edu;
stancil@physast.uga.edu; cravens@ku.edu; carey.lisse@jhuapl.edu;
adalgarno@cfa.harvard.edu
RI Lisse, Carey/B-7772-2016
OI Lisse, Carey/0000-0002-9548-1526
FU NASA Planetary Atmospheres Program [NNH07AF12I]
FX This work has been supported by NASA Planetary Atmospheres Program Grant
NNH07AF12I. We are also grateful to A. Bhardwaj and G. Branduardi-
Raymont for helpful discussions, and to the Chandra Helpdesk staff for
advice on and assistance with processing the raw observation files.
NR 37
TC 15
Z9 15
U1 3
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2009
VL 702
IS 2
BP L158
EP L162
DI 10.1088/0004-637X/702/2/L158
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BN
UT WOS:000269245500013
ER
PT J
AU Sanchez-Azofeifa, GA
Kalacska, M
do Espirito-Santo, MM
Fernandes, GW
Schnitzer, S
AF Arturo Sanchez-Azofeifa, G.
Kalacska, Margaret
do Espirito-Santo, Mario Marcos
Fernandes, G. Wilson
Schnitzer, Stefan
TI Tropical dry forest succession and the contribution of lianas to wood
area index (WAI)
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Canopy ecology; Leaf area index; Light; Tropical ecology; Succession
ID LEAF-AREA; RAIN-FOREST; LIGHT AVAILABILITY; AMAZONIAN BOLIVIA;
SEASONAL-CHANGES; LAI PRODUCTS; COSTA-RICA; TREES; DIVERSITY;
REGENERATION
AB The transmission and interception of light through the canopy is an important indicator of forest productivity in tropical forest ecosystems, and the amount of light that eventually reaches the forest floor is influenced by its interactions with leaves, branches, fruits, and flowers among many different canopy elements. While most studies of forest canopy light interception focus on leaf area index (LAI), very few studies have examined wood area index (WAI), which may account for a substantial component of light interception in tropical forests. The influence of lianas on the interception of light and their overall contribution to WAI is a potentially important factor, but it is generally overlooked because of its difficulty to assess. In this paper we evaluate the relative contribution that lianas have to the overall WAI and canopy openness as function of successional stage via a latitudinal comparison of sites across the Americas (Mexico, Costa Rica and Brazil). Our results suggest that lianas significantly increase WAI and decreases canopy openness. However, lianas were absent at all of our study sites where canopy openness exceeded 60%. Our data are the first to explicitly document the role of lianas in the estimation of WAI and, overall, they will contribute to better estimations of ecosystem level LAI in tropical environments, where there is a lack of data on WAI. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Arturo Sanchez-Azofeifa, G.; Kalacska, Margaret] Univ Alberta, Earth Observat Syst Lab, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[do Espirito-Santo, Mario Marcos] Univ Estadual Montes Claros, CCBS, Dept Biol Geral, Montes Claros, MG, Brazil.
[Fernandes, G. Wilson] Univ Fed Minas Gerais, ICB, Ecol Evolut & Biodiversidade DBG, BR-30161970 Belo Horizonte, MG, Brazil.
[Schnitzer, Stefan] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA.
[Arturo Sanchez-Azofeifa, G.; Schnitzer, Stefan] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Sanchez-Azofeifa, GA (reprint author), Univ Alberta, Earth Observat Syst Lab, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
EM arturo.sanchez@ualberta.ca
RI do Espirito Santo, Mario/O-4813-2014;
OI do Espirito Santo, Mario/0000-0001-8274-3075; Schnitzer,
Stefan/0000-0002-2715-9455; Kalacska, Margaret/0000-0002-1676-481X
FU Inter-American Institute for Global Change Research (IAI) CRN II [021];
US National Science Foundation [GEO-0452325]; Fundacao de Amparo a
Pesquisa de Minas Gerais (FAPEMIG) [CRA 2288/07]; Mexico's
SEMARNAT-CONACYT
FX This work was carried out with the aid of a grant from the
Inter-American Institute for Global Change Research (IAI) CRN II - 021,
which is supported by the US National Science Foundation (Grant
GEO-0452325). We are also grateful for the financial support provided by
Fundacao de Amparo a Pesquisa de Minas Gerais (FAPEMIG CRA 2288/07), as
well as Mexico's SEMARNAT-CONACYT under the CIEco-MABOTRO project. We
also thank Roger Blanco and Maria Marta Chavarria from the Santa Rosa
National Park, Dr. Eugenio Gonzalez and Mauricio Castillo from the Palo
Verde National Park for their logistical support as well as Ulises
Chavarria (Costa Rica), Roberto Espinoza (Costa Rica), Alfredo Pe rez
(Mexico), Mauricio Quesada (Mexico) and Gumersindo Sanchez (Mexico).
Finally, we would like to thank all the field assistants from the
University of Alberta, the Instituto Tecnologico de Costa Rica, the
Centro de Investigaciones en Ecosistemas (CIECO), Universidad Nacional
Autonoma de Mexico, and Universidade Estadual de Montes Claros - MG,
Brazil, for their help in data collection.
NR 53
TC 13
Z9 13
U1 5
U2 34
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD SEP 5
PY 2009
VL 258
IS 6
BP 941
EP 948
DI 10.1016/j.foreco.2008.10.007
PG 8
WC Forestry
SC Forestry
GA 495ES
UT WOS:000269874000006
ER
PT J
AU Cardoso, P
Aranda, SC
Lobo, JM
Dinis, F
Gaspar, C
Borges, PAV
AF Cardoso, Pedro
Aranda, Silvia C.
Lobo, Jorge M.
Dinis, Francisco
Gaspar, Clara
Borges, Paulo A. V.
TI A spatial scale assessment of habitat effects on arthropod communities
of an oceanic island
SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY
LA English
DT Article
DE Connectivity; Dispersal; Endemic species; Exotic plantations; Habitat
heterogeneity; Introduced species; Land-use; Landscape matrix;
Macaronesia; Native species
ID SPECIES-RICHNESS PATTERNS; FRAGMENTED LANDSCAPE; PLANTATION FORESTS;
RESOURCE SELECTION; REGIONAL SCALES; NATIVE FOREST; DIVERSITY;
BIODIVERSITY; AZORES; MATRIX
AB Most habitats in the Azores have undergone substantial land-use changes and anthropogenic disturbance during the last six centuries. In this study we assessed how the richness, abundance and composition of arthropod communities change with: (I) habitat type and (2) the surrounding land-use at different spatial scales. The research was conducted in Terceira Island, Azores. In eighty-one sites of four different habitat types (natural and exotic forests, semi-natural and intensively managed pastures), epigaeic arthropods were captured with pitfall traps and classified as endemic, native or introduced. The land-use surrounding each site was characterized within a radius ranging from 100 to 5000 m. Nonparametric tests were used to identify differences in species richness, abundance and composition between habitat types at different spatial scales. Endemic and native species were more abundant in natural forests, while introduced species were more abundant in intensively managed pastures. Natural forests and intensively managed pastures influenced arthropod species richness and composition at all spatial scales. Exotic forests and semi-natural pastures, however, influenced the composition of arthropod Communities at larger scales, promoting the connectivity of endemic and native species populations. Local species richness, abundance and composition of arthropod communities are mostly determined by the presence of nearby natural forests and/or intensively managed pastures. However, semi-natural pastures and exotic forests seem to play an important role as corridors between natural forests for both endemic and native species. Furthermore, exotic forests may serve as a refuge for some native species. (C) 2009 Elsevier Masson SAS. All rights reserved.
C1 [Cardoso, Pedro; Aranda, Silvia C.; Dinis, Francisco; Gaspar, Clara; Borges, Paulo A. V.] Univ Azores, Dept Agr Sci, CITA A Azorean Biodivers Grp, P-9701851 Angra Do Heroismo, Portugal.
[Aranda, Silvia C.; Lobo, Jorge M.] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain.
RP Cardoso, P (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 105,Room E-509, Washington, DC 20013 USA.
EM pcardoso@ennor.org
RI Borges, Paulo/B-2780-2008; Lobo, Jorge/E-2309-2013; Cardoso,
Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Lobo, Jorge/0000-0002-3152-4769;
Cardoso, Pedro/0000-0001-8119-9960
FU Direccao Regional da Ciencia e Tecnologia dos Acores [M112/F/014/2007,
M311/1009A/2005]; Fundacao para a Ciencia e Tecnologia
[SFRH/BD/13197/2003, SFRH/BD/11049/2002]; Direccao Regional dos Recursos
Florestais (Secretaria Regional da Agricultura e Pescas) [17.01-080203];
Spanish Ministry of Education and Science [CGL 2006-10196]
FX Many thanks go to Isabel R. Amorim for her most useful comments and
extensive English editing. PC and SA were supported by grants from
Direccao Regional da Ciencia e Tecnologia dos Acores (M112/F/014/2007
and M311/1009A/2005 respectively). FD and CG were supported by grants
from Fundacao para a Ciencia e Tecnologia (SFRH/BD/13197/2003 and
SFRH/BD/11049/2002 respectively). Funding for fieldwork was provided by
Direccao Regional dos Recursos Florestais (Secretaria Regional da
Agricultura e Pescas) through the project "Reservas Florestais dos
Acores: Cartografia e Inventariacao dos Artropodes Endemicos dos Acores"
(PROJ. 17.01-080203). We are also grateful for the financial support of
the Spanish Ministry of Education and Science (project CGL 2006-10196).
NR 70
TC 29
Z9 30
U1 0
U2 11
PU GAUTHIER-VILLARS/EDITIONS ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75015 PARIS, FRANCE
SN 1146-609X
J9 ACTA OECOL
JI Acta Oecol.-Int. J. Ecol.
PD SEP-OCT
PY 2009
VL 35
IS 5
BP 590
EP 597
DI 10.1016/j.actao.2009.05.005
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 506BP
UT WOS:000270748300004
ER
PT J
AU Averianov, A
Sues, HD
AF Averianov, Alexander
Sues, Hans-Dieter
TI First record of a basal neoceratopsian dinosaur from the Late Cretaceous
of Kazakhstan
SO ACTA PALAEONTOLOGICA POLONICA
LA English
DT Article
ID ARAL SEA REGION; CERATOPSIAN DINOSAUR; CHINA
AB The oldest known ceratopsians come from the Late Jurassic of China (Zhao et al. 1999; Xu et al. 2006). During the Early Cretaceous, the basal ceratopsian Psittacosaurus was among the most common dinosaurs in Asia but more derived basal neoceratopsians were quite rare on that continent (Xu et al. 2002; Makovicky and Norell 2006). Basal neoceratopsians became more abundant in the Late Cretaceous of Mongolia and China, although they are not known in this region from the latest Cretaceous (You and Dodson 2004; Alifanov 2008). In contrast, basal neoceratopsians are rare during the Early Cretaceous in North America but became common and diverse during the Campanian and Maastrichtian (You and Dodson 2004; Chinnery and Horner 2007). Little is known about the evolutionary history of this group in more inland regions of what are now Kazakhstan and adjoining countries. Asiaceratops documents the presence of basal neoceratopsians in the Cenomanian of Uzbekistan (Nessov et al. 1989). Here we report on the first record of a basal neoceratopsians in the Late Cretaceous of Kazakhstan, based on two cranial bones from the Turonian Zhirkindek Formation in the northeastern Aral Sea region.
C1 [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia.
[Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Averianov, A (reprint author), Russian Acad Sci, Inst Zool, Univ Skaya Nab 1, St Petersburg 199034, Russia.
EM lepus@zin.ru; suesh@si.edu
RI Averianov, Alexander/M-8490-2013
OI Averianov, Alexander/0000-0001-5948-0799
FU US Civilian Research and Development Foundation [RUB1-2860-ST-07]
FX are grateful to Brenda J. Chinnery-Allgeier (University of Texas at
Austin, USA), David C. Evans (Royal Ontario Museum, Ottawa, Canada), and
Michael J. Ryan (Cleveland Museum of Natural History, Cleveland, USA)
for review of the manuscript and helpful suggestions. This work was
supported by US Civilian Research and Development Foundation grant
RUB1-2860-ST-07 to AA and J. David Archibald.
NR 20
TC 4
Z9 5
U1 0
U2 3
PU INST PALEOBIOLOGII PAN
PI WARSAW
PA UL TWARDA 51/55, 00-818 WARSAW, POLAND
SN 0567-7920
J9 ACTA PALAEONTOL POL
JI Acta Palaeontol. Pol.
PD SEP
PY 2009
VL 54
IS 3
BP 553
EP 556
DI 10.4202/app.2008.0079
PG 4
WC Paleontology
SC Paleontology
GA 503XD
UT WOS:000270574400017
ER
PT J
AU Solis, MA
Metz, MA
Janzen, DH
AF Solis, M. Alma
Metz, Mark A.
Janzen, Daniel H.
TI Phylogenetic Analysis of Cosmopterosis (Lepidoptera: Crambidae:
Glaphyriinae) With Discussions on Male Secondary Sexual Characters and
Larval Feeding on Capparis (Capparaceae) in the Pyraloidea and
Lepidoptera (Insecta)
SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA
LA English
DT Article
DE Pyraloidea; systematics; larval morphology; Costa Rica; Capparaceae
ID PYRALIDAE; GENERA; SYSTEMATICS; MORPHOLOGY; GENUS
AB New species of Cosmopterosis Amsel were discovered feeding on Capparis L. (Capparaceae) during exploration for caterpillars in the Area de Conservacion Guanacaste (ACG), Costa Rica. Cosmopterosis is revised and now includes four species. Three new species, C. hispida, C. jasonhalli, and C. spatha, and the immatures of C. spatha and biology for two species, C. jasonhalli and C. spatha, are described; the type species, C. thetysalis (Walker), is redescribed. A key and illustrations for the identification of the species is provided. We propose a hypothesis for the relationship between species in Cosmopterosis and the placement of Cosmopterosis in the subfamily. The cladistic analysis, the first such analysis in the Glaphyriinae, included 21 morphological characters one of which, the radiodiscal process, a male secondary sexual character and presumably an androconial scent pouch is described and considered a autapomorphy for the genus. Male secondary sexual characters and larval feeding on Capparis in Pyraloidea and Lepidoptera is discussed.
C1 [Solis, M. Alma; Metz, Mark A.] USDA, SEL, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Janzen, Daniel H.] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA.
RP Solis, MA (reprint author), USDA, SEL, Smithsonian Inst, Natl Museum Nat Hist, POB 37012,E-517,MRC 168, Washington, DC 20013 USA.
EM alma.solis@ars.usda.gov
FU National Science Foundation [BSR 90-24770, DEB 93-06296, DEB 94-00829,
DEB 97-05072, DEB 00-72730, DEB 05-15699]; Area de Conservacion
Guanacaste, Consejo Nacional para Investigaciones Cientificas y
Tecbnologicas (CONICIT); INBio
FX We thank various individuals worldwide who care for Pyraloidea
collections and assisted our search for material, but especially K. Tuck
(BMNH), E. J. van Nieurkerken (RMNH) M. Wall (SDNHM), E. Phillips
(formerly with INBio), and V. O. Becker who provided extensive material
from Brazil from his personal collection. We thank E. Araya, C. Cano, E.
Cantillano, M. Carmona, O. Espinosa, R. Espinosa, R. Frauco, D. Garcia,
W. Hallwachs, C. Moraga, R. Moraga, G. Pereira, M. Pereira, J. Perez, F.
Quesada, H. Ramirez, L Rios, P. Rios, G. Sihezar, and F. Vargas for
caterpillar hunting and husbandry; R. Espinosa, J. Gonzales, A.
Guadamuz, B. Hammel, N. Zamora, and the herbarium staff at INBio for
foodplant identifications; and S. R. Shaw, J. B. Whitfield and D. M.
Wood for wasp and fly identifications. We thank Shen-Horn Yen (National
Sun Yat-Sen University, Taiwan) and F. Christian Thompson, Tom Henry,
John Brown (SEL, USDA) for helpful suggestions on the manuscript.
Special thanks to Thomas Simonsen who provided a rigorous review that
only a true morphologist could do. The ACG caterpillar inventory has
been variously supported by National Science Foundation grants BSR
90-24770, DEB 93-06296, DEB 94-00829, DEB 97-05072, DEB 00-72730, and
DEB 05-15699 and by Area de Conservacion Guanacaste, Consejo Nacional
para Investigaciones Cientificas y Tecbnologicas (CONICIT), INBio, and
the government of Costa Rica.
NR 57
TC 2
Z9 2
U1 0
U2 2
PU ENTOMOLOGICAL SOC AMER
PI LANHAM
PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA
SN 0013-8746
J9 ANN ENTOMOL SOC AM
JI Ann. Entomol. Soc. Am.
PD SEP
PY 2009
VL 102
IS 5
BP 766
EP 784
PG 19
WC Entomology
SC Entomology
GA 493DT
UT WOS:000269714300004
ER
PT J
AU Cockell, CS
Kaltenegger, L
Raven, JA
AF Cockell, Charles S.
Kaltenegger, Lisa
Raven, John A.
TI Cryptic Photosynthesis-Extrasolar Planetary Oxygen Without a Surface
Biological Signature
SO ASTROBIOLOGY
LA English
DT Review
DE Atmospheric gases; Bioastronomy; Extrasolar terrestrial planets;
Photosynthesis; Planetary atmospheres
ID DEEP CHLOROPHYLL MAXIMUM; PLATELET ICE ECOSYSTEM; DENSE MICROALGAL
BLOOM; ANTARCTIC SEA-ICE; SOIL CRUSTS; POLAR DESERT; CRYPTOENDOLITHIC
CYANOBACTERIA; ENDOLITHIC CYANOBACTERIA; MICROBIAL COMMUNITY; SPECTRAL
SIGNATURES
AB On Earth, photosynthetic organisms are responsible for the production of virtually all the oxygen in the atmosphere. On land, vegetation reflects in the visible and leads to a "red edge,'' which developed about 450 million years ago on Earth and has been proposed as a biosignature for life on extrasolar planets. However, in many regions on Earth, particularly where surface conditions are extreme - in hot and cold deserts, for example - photosynthetic organisms can be driven into and under substrates where light is still sufficient for photosynthesis. These communities exhibit no detectable surface spectral signature to indicate life. The same is true of the assemblages of photosynthetic organisms at more than a few meters' depth in water bodies. These communities are widespread and dominate local photosynthetic productivity. We review known cryptic photosynthetic communities and their productivity. We have linked geomicrobiology with observational astronomy by calculating the disk-averaged spectra of cryptic habitats and identifying detectable features on an exoplanet dominated by such a biota. The hypothetical cryptic photosynthesis worlds discussed here are Earth analogues that show detectable atmospheric biosignatures like our own planet but do not exhibit a discernable biological surface feature in the disc-averaged spectrum.
C1 [Cockell, Charles S.] Open Univ, Ctr Earth Planetary Space & Astron Res, Milton Keynes MK7 6AA, Bucks, England.
[Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Raven, John A.] Univ Dundee, Scottish Crop Res Inst, Div Plant Sci, Dundee, Scotland.
RP Cockell, CS (reprint author), Open Univ, Ctr Earth Planetary Space & Astron Res, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
EM C.S.Cockell@open.ac.uk
FU Science and Technology Facilities Council (STFC); The University of
Dundee is a registered Scottish Charity [SC015096]
FX Charles Cockell gratefully acknowledges support from the Science and
Technology Facilities Council (STFC). Lisa Kaltenegger gratefully
acknowledges support from the Origin of Life Initiative and the NASA
Astrobiology Institute. John Raven gratefully acknowledges discussion
with Professor Lyn Jones on the evolution of infrared reflectivity in
photosynthetic organisms on land. The University of Dundee is a
registered Scottish Charity, No. SC015096.
NR 133
TC 15
Z9 16
U1 2
U2 14
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2009
VL 9
IS 7
BP 623
EP 636
DI 10.1089/ast.2008.0273
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 498JE
UT WOS:000270134600003
PM 19778274
ER
PT J
AU Currie, T
Kenyon, SJ
AF Currie, Thayne
Kenyon, Scott J.
TI DEEP MIPS OBSERVATIONS OF THE IC 348 NEBULA: CONSTRAINTS ON THE
EVOLUTIONARY STATE OF ANEMIC CIRCUMSTELLAR DISKS AND THE
PRIMORDIAL-TO-DEBRIS DISK TRANSITION
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (IC 348); planetary systems:
formation; planetary systems: protoplanetary disks; stars:
pre-main-sequence
ID LOW-MASS STARS; TERRESTRIAL PLANET FORMATION; SPECTRAL
ENERGY-DISTRIBUTIONS; SCORPIUS OB ASSOCIATION; SPITZER-SPACE-TELESCOPE;
YOUNG STELLAR OBJECTS; MAIN-SEQUENCE TRACKS; GAS GIANT PLANETS; CLUSTER
IC-348; TAURUS-AURIGA
AB We describe new, deep MIPS photometry and new high signal-to-noise optical spectroscopy of the 2.5 Myr old IC 348 Nebula. To probe the properties of the IC 348 disk population, we combine these data with previous optical/infrared photometry and spectroscopy to identify stars with gas accretion, to examine their mid-IR colors, and to model their spectral energy distributions. IC 348 contains many sources in different evolutionary states, including protostars and stars surrounded by primordial disks, two kinds of transitional disks, and debris disks. Most disks surrounding early/intermediate spectral-type stars (>1.4 M-circle dot at 2.5 Myr) are debris disks; most disks surrounding solar and subsolar-mass stars are primordial disks. At the 1-2 sigma level, more massive stars also have a smaller frequency of gas accretion and smaller mid-IR luminosities than lower-mass stars. These trends are suggestive of a stellar mass-dependent evolution of disks, where most disks around high/intermediate-mass stars shed their primordial disks on rapid, 2.5 Myr timescales. The frequency of MIPS-detected transitional disks is approximate to 15%-35% for stars plausibly more massive than 0.5 M-circle dot. The relative frequency of transitional disks in IC 348 compared to that for 1 Myr old Taurus and 5 Myr old NGC 2362 is consistent with a transition timescale that is a significant fraction of the total primordial disk lifetime.
C1 [Currie, Thayne; Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA.
EM tcurrie@cfa.harvard.edu; skenyon@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X
NR 71
TC 39
Z9 39
U1 0
U2 1
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 SEP
PY 2009
VL 138
IS 3
BP 703
EP 726
DI 10.1088/0004-6256/138/3/703
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 490OF
UT WOS:000269509700001
ER
PT J
AU Hodge, PW
Krienke, OK
Bellazzini, M
Perina, S
Barmby, P
Cohen, JG
Puzia, TH
Strader, J
AF Hodge, P. W.
Krienke, O. K.
Bellazzini, M.
Perina, S.
Barmby, P.
Cohen, J. G.
Puzia, T. H.
Strader, J.
TI AN HST/WFPC SURVEY OF BRIGHT YOUNG CLUSTERS IN M31. II. PHOTOMETRY OF
LESS LUMINOUS CLUSTERS IN THE FIELDS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 224, M31, Andromeda); galaxies: star clusters;
galaxies: stellar content; Local Group
ID SPACE-TELESCOPE SURVEY; SMALL-MAGELLANIC-CLOUD; STAR-CLUSTERS; WFPC2;
POPULATION; POINTINGS; CATALOG
AB We report on the properties of 89 low-mass star clusters located in the vicinity of luminous young clusters ("blue globulars") in the disk of M31. Eighty-two of the clusters are newly detected. We have determined their integrated magnitudes and colors, based on a series of Hubble Space Telescope (HST)/Wide Field Planetary Camera 2 exposures in blue and red (HST filters F450W and F814W). The integrated apparent magnitudes range from F450W = 17.5 to 22.5, and the colors indicate a wide range of ages. Stellar color-magnitude diagrams for all clusters were obtained and those with bright enough stars were fit to theoretical isochrones to provide age estimates. The ages range from 12 Myr to >500 Myr. Reddenings, which average E(F450 - F814) = 0.59 with a dispersion of 0.21 mag, were derived from the main-sequence fitting for those clusters. Comparison of these ages and integrated colors with single population theoretical models with solar abundances suggests a color offset of 0.085 mag at the ages tested. Estimated ages for the remaining clusters are based on their measured colors. The age-frequency diagram shows a steep decline of number with age, with a large decrease in number per age interval between the youngest and the oldest clusters detected.
C1 [Hodge, P. W.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Krienke, O. K.] Seattle Pacific Univ, Seattle, WA 98119 USA.
[Bellazzini, M.; Perina, S.] INAF Osservatorio Bologna, I-40127 Bologna, Italy.
[Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cohen, J. G.] CALTECH, Palomar Observ, Pasadena, CA 91125 USA.
[Puzia, T. H.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
RP Hodge, PW (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RI Bellazzini , Michele/O-9373-2015; Barmby, Pauline/I-7194-2016
OI Bellazzini , Michele/0000-0001-8200-810X; Barmby,
Pauline/0000-0003-2767-0090
FU NASA [NAS 5-26555]; [GOI-10818]
FX This paper was based on observations made with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc. under
NASA contract NAS 5-26555. These observations are associated with
program GOI-10818 (PI: J. G. Cohen) and were partially funded under that
program.
NR 18
TC 10
Z9 10
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2009
VL 138
IS 3
BP 770
EP 779
DI 10.1088/0004-6256/138/3/770
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 490OF
UT WOS:000269509700004
ER
PT J
AU Baxter, EJ
Covey, KR
Muench, AA
Furesz, G
Rebull, L
Szentgyorgyi, AH
AF Baxter, Eric J.
Covey, Kevin R.
Muench, August A.
Furesz, Gabor
Rebull, Luisa
Szentgyorgyi, Andrew H.
TI THE DISTANCE TO NGC 2264
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: statistical; open clusters and associations: individual (NGC
2264); stars: distances; stars: formation; stars: rotation
ID ORION-NEBULA-CLUSTER; T-TAURI STARS; LOW-MASS STARS; MAIN-SEQUENCE
STARS; YOUNG OPEN CLUSTERS; M-DWARFS; RADIAL-VELOCITIES; INFRARED
COLORS; FORMING REGION; AGE SPREADS
AB We determine the distance to the open cluster NGC 2264 using a statistical analysis of cluster member inclinations. We derive distance-dependent values of sin i (where i is the inclination angle) for 97 stars in NGC 2264 from the rotation periods, luminosities, effective temperatures, and projected equatorial rotation velocities, v sin i, measured for these stars. We have measured 96 of the v sin i values in our sample by analyzing high-resolution spectra with a cross-correlation technique. We model the observed distribution of sin i for the cluster by assuming that member stars have random axial orientations and by adopting prescriptions for the measurement errors in our sample. By adjusting the distance assumed in the observed sin i distribution until it matches the modeled distribution, we obtain a best-fit distance for the cluster. We find the data to be consistent with a distance to NGC 2264 of 913 pc. Quantitative tests of our analysis reveal uncertainties of 40 and 110 pc due to sampling and systematic effects, respectively. This distance estimate suggests a revised age for the cluster of similar to 1.5 Myr, although more detailed investigations of the full cluster membership are required to draw strong conclusions.
C1 [Baxter, Eric J.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Covey, Kevin R.; Muench, August A.; Furesz, Gabor; Szentgyorgyi, Andrew H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rebull, Luisa] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Baxter, EJ (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
OI Muench, August/0000-0003-0666-6367; Rebull, Luisa/0000-0001-6381-515X;
Covey, Kevin/0000-0001-6914-7797
FU NSF; NASA [1335523]; Spitzer Space Telescope Fellowship Program
FX The authors thank Steve Strom for a prompt and helpful referee report
that improved the analysis presented here, and Russel White and Javed
Gabor for providing IDL code that formed the basis of our
cross-correlation pipeline. E. J. B. acknowledges the support of the SAO
Summer Intern Program, made possible by a grant from the NSF. NASA
support was provided to K. R. C. for this work through the Spitzer Space
Telescope Fellowship Program, through a contract issued by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. A. A. M. was supported by NASA through contract
1335523 issued by JPL/Caltech.
NR 46
TC 38
Z9 38
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2009
VL 138
IS 3
BP 963
EP 974
DI 10.1088/0004-6256/138/3/963
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 490OF
UT WOS:000269509700023
ER
PT J
AU Braito, V
Reeves, JN
Della Ceca, R
Ptak, A
Risaliti, G
Yaqoob, T
AF Braito, V.
Reeves, J. N.
Della Ceca, R.
Ptak, A.
Risaliti, G.
Yaqoob, T.
TI A Suzaku observation of the ULIRG IRAS19254-7245: discerning the AGN
component
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: individual: IRAS 19254-7245; galaxies:
Seyfert; X-rays: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; STAR-FORMATION
RATE; X-RAY-SPECTRA; BRIGHT SERENDIPITOUS SURVEY; FORMATION RATE
INDICATOR; XMM-NEWTON OBSERVATIONS; 2-10 KEV LUMINOSITY; BLACK-HOLES;
STARBURST GALAXIES
AB We discuss a long Suzaku observation of IRAS 19254-7245 (also known as the Superantennae), one of the brightest and well studied Ultra Luminous Infrared Galaxies in the local Universe.
This long observation provided the first detection of IRAS 19254-7245 above 10 keV, and a measurement of a 15-30 keV flux of similar to 5 x 10(-12) erg cm(-2) s(-1). The detection above 10 keV has allowed us to determine, for the first time, the intrinsic luminosity of the AGN hosted in IRAS 19254-7245, which is strongly absorbed (N-H similar to 3 x 10(24) cm(-2)) and has an intrinsic luminosity (L(2 - 10 keV) similar to 3 x 10(44) erg s(-1)) in the QSO regime.
The 2-10 keV spectrum of IRAS 19254-7245 is remarkably hard (Gamma similar to 1.2), and presents a strong iron line (EW similar to 0.7 keV), clearly suggesting that below 10 keV we observe only reprocessed radiation. Since the energy of the Fe K emission is found to be similar to 6.7 keV, consistent with He-like Fe, and its EW is too high to be explained by a starburst-dominated scenario, we suggest that the 2-10 keV emission of IRAS 19254-7245 is dominated by reflection/scattering from highly ionized matter. Within this latter scenario, we found that the photon index of the illuminating source is Gamma = 1.87(-0.28)(+0.11) in excellent agreement with the mean value found for radio quiet unobscured AGN.
C1 [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Braito, V.; Reeves, J. N.; Ptak, A.; Yaqoob, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Della Ceca, R.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy.
[Ptak, A.; Yaqoob, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Braito, V (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM bv67@star.le.ac.uk
RI Ptak, Andrew/D-3574-2012; XRAY, SUZAKU/A-1808-2009;
OI Risaliti, Guido/0000-0002-3556-977X; Della Ceca,
Roberto/0000-0001-7551-2252; Braito, Valentina/0000-0002-2629-4989
FU UK STFC research council; ASI (Agenzia Spaziale Italiana) [I/088/06/0];
National Aeronautics and Space Administration through the NASA
[NNG04GB78A]
FX V. B. acknowledge support from the UK STFC research council. R. D. C.
acknowledge financial support from the ASI (Agenzia Spaziale Italiana)
grant I/088/06/0. Support for this work was provided by the National
Aeronautics and Space Administration through the NASA grant NNG04GB78A.
We thank the anonymous referee for his/her useful comments, which have
improved this paper.
NR 49
TC 13
Z9 13
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 SEP
PY 2009
VL 504
IS 1
BP 53
EP 59
DI 10.1051/0004-6361/200811516
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HU
UT WOS:000269728200006
ER
PT J
AU Fallscheer, C
Beuther, H
Zhang, Q
Keto, E
Sridharan, TK
AF Fallscheer, C.
Beuther, H.
Zhang, Q.
Keto, E.
Sridharan, T. K.
TI Rotational structure and outflow in the infrared dark cloud 18223-3
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; stars: individual: IRDC 18223-3; stars: early-type
ID MASS PROTOSTELLAR CANDIDATES; ULTRACOMPACT HII-REGIONS; ACCRETION DISK;
STAR-FORMATION; CO OUTFLOWS; EMISSION; SEARCH; SYSTEM; SAMPLE; SHOCKS
AB Aims. We examine an Infrared Dark Cloud (IRDC) at high spatial resolution as a means to study rotation, outflow, and infall at the onset of massive star formation.
Methods. The IRDC 18223-3 was observed at 1.1 mm and 1.3 mm with the Submillimeter Array (SMA) and follow-up short spacing information was obtained with the IRAM 30m telescope. Additional data were taken at 3 mm with the IRAM Plateau de Bure interferometer (PdBI).
Results. Submillimeter Array observations combined with IRAM 30 m data in (12)CO(2-1) reveal the outflow orientation in the IRDC 18223-3 region, and PdBI 3 mm observations confirm this orientation in other molecular species. The implication of the outflow's presence is that an accretion disk is feeding it, so using line data for high density tracers such as C(18)O, N(2)H(+), and CH(3)OH, we looked for indications of a velocity gradient perpendicular to the outflow direction. Surprisingly, this gradient turns out to be most apparent in CH(3)OH. The large size (28000 AU) of the flattened rotating object detected indicates that this velocity gradient cannot be due solely to a disk, but rather from inward spiraling gas within which a Keplerian disk likely exists. The rotational signatures can be modeled via rotationally infalling gas. From the outflow parameters, we derive properties of the source such as an outflow dynamical age of similar to 37000 years, outflow mass of similar to 13 M(circle dot), and outflow energy of similar to 1.7 x 10(46) erg. While the outflow mass and energy are clearly consistent with a high-mass star forming region, the outflow dynamical age indicates a slightly more evolved evolutionary stage than previous spectral energy distribution (SED) modeling indicates.
Conclusions. The orientation of the molecular outflow associated with IRDC 18223-3 is in the northwest-southeast direction and velocity gradients orthogonal to the outflow reveal a large rotating structure likely harboring an accretion disk within. We also present a model of the observed methanol velocity gradient. The calculated outflow properties reveal that this is truly a massive star in the making. These data present evidence for one of the youngest known outflow/infall/disk systems in massive star formation. A tentative evolutionary picture for massive disks is discussed.
C1 [Fallscheer, C.; Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Zhang, Q.; Keto, E.; Sridharan, T. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fallscheer, C (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM fallscheer@mpia.de
OI Zhang, Qizhou/0000-0003-2384-6589
FU Deutsche Forschungsgemeinschaft [BE 2578]; International Max-Planck
Research School for Astronomy Cosmic Physics
FX C. F. and H. B. acknowledge support by the Deutsche
Forschungsgemeinschaft, DFG project number BE 2578. C. F. also
acknowledges support from the International Max-Planck Research School
for Astronomy & Cosmic Physics at the University of Heidelberg and
thanks Jan Martin Winters for his guidance in reducing the PdBI data
sets. We express our gratitude to the anonymous referee for his/her
constructive comments which improved the paper.
NR 38
TC 23
Z9 23
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2009
VL 504
IS 1
BP 127
EP 137
DI 10.1051/0004-6361/200912307
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HU
UT WOS:000269728200015
ER
PT J
AU Purcell, CR
Minier, V
Longmore, SN
Andre, P
Walsh, AJ
Jones, P
Herpin, F
Hill, T
Cunningham, MR
Burton, MG
AF Purcell, C. R.
Minier, V.
Longmore, S. N.
Andre, Ph.
Walsh, A. J.
Jones, P.
Herpin, F.
Hill, T.
Cunningham, M. R.
Burton, M. G.
TI Multi-generation massive star-formation in NGC 3576
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; stars: formation; HII regions; radio lines: ISM; ISM:
abundances; stars: pre-main-sequence
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MOLECULAR CLOUD
CORES; INFRARED DARK CLOUDS; H-II REGIONS; H2O MASERS; INTERSTELLAR
AMMONIA; HYPERFINE-STRUCTURE; FORMING REGIONS; INVERSION TRANSITION
AB Context. Recent 1.2-mm continuum observations have shown the giant H II region NGC 3576 to be embedded in the centre of an extended filamentary dust-cloud. The bulk of the filament away from the H II region contains a number of clumps seen only at (sub-)millimetre wavelengths. Infrared and radio observations of the central star cluster have uncovered evidence of sequential star-formation leading us to believe that the adjacent clumps may host massive protostellar objects at a very early stage of evolution.
Aims. We have investigated the physical and chemical conditions in the dusty clumps with the goal of characterising their star-forming content.
Methods. We have used the Australia Telescope Compact Array (ATCA) to image the cloud for the NH(3) (1,1), (2,2) and (4,4) transitions, 22 GHz H(2)O masers, and 23 GHz continuum emission. The 70-m Tidbinbilla dish was used to estimate the total integrated intensity of NH(3). We also utilised the 22-m Mopra antenna to map the region for the molecular lines (13)CO (1-0), C(18)O (1-0), HCO(+) (1-0), H(13)CO(+) (1-0), CS (1-0) and N(2)H(+) (1-0).
Results. Emission from dense molecular gas follows the morphology of the 1.2-mm dust emission, except towards the central ionised region. The H II region is observed to be expanding into the molecular cloud, sweeping up a clumpy shell of gas, while the central star cluster is dispersing the molecular gas to the east. Analysis of the NH(3) data indicates that temperature and linewidth gradients exist in the western arm of the filament. Temperatures are highest adjacent to the central H II region, indicating that the embedded cluster of young stars there is heating the gas. Six new H(2)O masers were detected in the arms of the filament, all associated with NH(3) emission peaks, confirming that star-formation has begun within these cores. Core masses range from 5 to 516 M(circle dot) and most appear to be gravitationally bound. Complementary results by Andre et al. (2008) imply that seven cores will go on to form massive stars between 15 and 50 M(circle dot). The large scale velocity structure of the filament is smooth, but at least one clump shows the signature of inward gas motions via asymmetries in the NH(3) (1,1) line profiles. The same clump exhibits an enhanced abundance of N(2)H(+), which coupled with an absence of CO indicates depletion onto the dust grain surface.
Conclusions. The HII region at the heart of NGC 3576 is potentially triggering the formation of massive stars in the bulk of the associated cloud.
C1 [Purcell, C. R.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Purcell, C. R.; Longmore, S. N.; Walsh, A. J.; Jones, P.; Hill, T.; Cunningham, M. R.; Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Minier, V.; Andre, Ph.] CEA, DSM, IRFU, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Minier, V.; Andre, Ph.] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,CEA DSM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Longmore, S. N.] CSIRO Australia Telescope Natl Facill, Epping, NSW 1710, Australia.
[Walsh, A. J.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia.
[Jones, P.] Univ Chile, Dept Astron, Santiago, Chile.
[Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, F-33000 Bordeaux, France.
[Herpin, F.] CNRS INSU, UMR 5804, F-33271 Floirac, France.
[Hill, T.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Hill, T.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Purcell, CR (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
EM cormac.purcell@manchester.ac.uk
RI Walsh, Andrew/B-5627-2013;
OI Walsh, Andrew/0000-0001-9506-0855; Purcell, Cormac/0000-0002-7491-7386;
Burton, Michael/0000-0001-7289-1998; Cunningham,
Maria/0000-0001-7020-6176
NR 76
TC 12
Z9 12
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2009
VL 504
IS 1
BP 139
EP 159
DI 10.1051/0004-6361/200811358
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HU
UT WOS:000269728200016
ER
PT J
AU Paggi, A
Massaro, F
Vittorini, V
Cavaliere, A
D'Ammando, F
Vagnetti, F
Tavani, M
AF Paggi, A.
Massaro, F.
Vittorini, V.
Cavaliere, A.
D'Ammando, F.
Vagnetti, F.
Tavani, M.
TI SSC radiation in BL Lacertae sources, the end of the tether
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: jets; BL Lacertae objects: general;
radiation mechanisms: non-thermal
ID LOG-PARABOLIC SPECTRA; GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI;
MULTIWAVELENGTH OBSERVATIONS; PARTICLE-ACCELERATION; ELECTRON
ACCELERATION; EXTRAGALACTIC SOURCES; OCTOBER 2007; TEV; ENERGY
AB Context. The synchrotron-self Compton (SSC) radiation process is widely held to provide a close representation of the double peaked spectral energy distributions from BL Lac Objects (BL Lacs). This subclass of Active Galactic Nuclei is marked by non-thermal beamed radiations, highly variable on timescales of days or less. Their outbursts in the. rays relative to the optical/X rays might be surmised to be enhanced in BL Lacs as these photons are upscattered via the inverse Compton (IC) process.
Aims. From the observed correlations among the spectral parameters (peak frequencies, fluxes and curvature) during optical/X-ray variations we aim at predicting corresponding correlations in the gamma-ray band, and the actual relations between the gamma-ray and the X-ray variability consistent with the SSC emission process.
Methods. We start from the homogeneous single-zone SSC source model, with log-parabolic energies distributions of emitting electron as required by the X-ray data of many sources. We find relations among spectral parameters of the IC radiation in both the Thomson (for Low energy BL Lacs) and the Klein-Nishina regimes (mainly for High energy BL Lacs); whence we compute how variability is driven by a smooth increase of key source parameters, primarily the root mean square electron energy.
Results. In the Klein-Nishina regime the model predicts for HBLs lower inverse Compton fluxes relative to synchrotron, and milder gamma-ray relative to X-ray variations. Stronger gamma-ray flares observed in some HBLs like Mrk 501 are understood in terms of additional, smooth increases also of the emitting electron density. However, episodes of rapid flares as recently reported at TeV energies are beyond the reach of the single component SSC model with one dominant varying parameter. Furthermore, spectral correlations at variance with our predictions, as well as TeV emissions in LBL objects (like BL Lacertae itself) cannot be explained in terms of the simple HSZ SSC model, and in these cases the source may require additional electron populations in more elaborate structures like decelerated relativistic outflows or sub-jet scenarios.
Conclusions. We provide a comprehensive benchmark to straightforwardly gauge the capabilities and effectiveness of the SSC radiation process. The single component SSC source model in the Thomson regime turns out to be adequate for many LBL sources. In the mild Klein-Nishina regime it covers HBL sources undergoing variations driven by smooth increase of a number of source parameters. However, the simple model meets its limits with the fast/strong flares recently reported for a few sources in the TeV range; these clearly require sudden accelerations of emitting electrons in a second source component.
C1 [Paggi, A.; Cavaliere, A.; D'Ammando, F.; Vagnetti, F.; Tavani, M.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Massaro, F.] Harvard Univ, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Vittorini, V.; D'Ammando, F.; Tavani, M.] INAF, I-00100 Rome, Italy.
RP Paggi, A (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy.
EM alessandro.paggi@roma2.infn.it
RI Vagnetti, Fausto/F-7130-2014; Massaro, Francesco/L-9102-2016; Paggi,
Alessandro/C-1219-2017;
OI Vagnetti, Fausto/0000-0002-6689-9317; Massaro,
Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410;
Tavani, Marco/0000-0003-2893-1459
FU Foundation BLANCEFLOR Boncompagni-Ludovisi
FX We thank our referee for useful comments and helpful suggestions. F.
Massaro acknowledges the Foundation BLANCEFLOR Boncompagni-Ludovisi, nee
Bildt, for the grant awarded him in 2009 to support his research.
NR 55
TC 21
Z9 23
U1 0
U2 5
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2009
VL 504
IS 3
BP 821
EP U15
DI 10.1051/0004-6361/200912237
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 498XZ
UT WOS:000270180600013
ER
PT J
AU Peng, EW
Jordan, A
Blakeslee, JP
Mieske, S
Cote, P
Ferrarese, L
Harris, WE
Madrid, JP
Meurer, GR
AF Peng, Eric W.
Jordan, Andres
Blakeslee, John P.
Mieske, Steffen
Cote, Patrick
Ferrarese, Laura
Harris, William E.
Madrid, Juan P.
Meurer, Gerhardt R.
TI THE COLOR-MAGNITUDE RELATION FOR METAL-POOR GLOBULAR CLUSTERS IN M87:
CONFIRMATION FROM DEEP HST/ACS IMAGING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: elliptical and lenticular, cD; galaxies:
evolution; galaxies: individual (M87); galaxies: star clusters; globular
clusters: general
ID ACS-VIRGO CLUSTER; EARLY-TYPE GALAXIES; TELESCOPE ADVANCED CAMERA;
LUMINOSITY FUNCTION; ELLIPTIC GALAXIES; GIANT ELLIPTICALS; HUBBLE
CONSTANT; STAR-CLUSTERS; SBF SURVEY; SYSTEMS
AB Metal-poor globular clusters (GCs) are our local link to the earliest epochs of star formation and galaxy building. Studies of extragalactic GC systems using deep, high-quality imaging have revealed a small but significant slope to the color-magnitude relation for metal-poor GCs in a number of galaxies. We present a study of the M87 GC system using deep, archival HST/ACS imaging with the F606W and F814W filters, in which we find a significant color-magnitude relation for the metal-poor GCs. The slope of this relation in the I versus V-I color-magnitude diagram (gamma(I) =-0.024 +/- 0.006) is perfectly consistent with expectations based on previously published results using data from the ACS Virgo Cluster Survey. The relation is driven by the most luminous GCs, those with M(I) less than or similar to -10, and its significance is largest when fitting metal-poor GCs brighter than M(I) = -7.8, a luminosity which is similar to 1 mag fainter than our fitted Gaussian mean for the luminosity function (LF) of blue, metalpoor GCs (similar to 0.8 mag fainter than the mean for all GCs). These results indicate that there is a mass scale at which the correlation begins, and is consistent with a scenario where self-enrichment drives a mass-metallicity relationship. We show that previously measured half-light radii of M87 GCs from best-fit PSF-convolved King models are consistent with the more accurate measurements in this study, and we also explain how the color magnitude relation for metal-poor GCs is real and cannot be an artifact of the photometry. We fit Gaussian and evolved Schechter functions to the luminosity distribution of GCs across all colors, as well as divided into blue and red subpopulations, finding that the blue GCs have a brighter mean luminosity and a narrower distribution than the red GCs. Finally, we present a catalog of astrometry and photometry for 2250 M87 GCs.
C1 [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Peng, Eric W.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Blakeslee, John P.; Cote, Patrick; Ferrarese, Laura] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Mieske, Steffen] European So Observ, Santiago 19, Chile.
[Harris, William E.; Madrid, Juan P.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Meurer, Gerhardt R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Peng, EW (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
EM peng@bac.pku.edu.cn
OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548
FU Peking University Hundred Talent Fund [985]; Chilean Center of
Excellence in Astrophysics and Associated Technologies; Chilean Center
for Astrophysics FONDAP [15010003]
FX We thank Soren Larsen for sharing his HST/WFPC2 photometry of M87 GCs.
E. W. P. gratefully acknowledges the support of the Peking University
Hundred Talent Fund (985). A. J. acknowledges support from the Chilean
Center of Excellence in Astrophysics and Associated Technologies, and
from the Chilean Center for Astrophysics FONDAP 15010003. This research
has made use of the NASA/IPAC Extragalactic Database (NED) which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 59
TC 53
Z9 53
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 42
EP 51
DI 10.1088/0004-637X/703/1/42
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000005
ER
PT J
AU Lada, CJ
Lombardi, M
Alves, JF
AF Lada, Charles J.
Lombardi, Marco
Alves, Joao F.
TI THE CALIFORNIA MOLECULAR CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: clouds; stars: formation
ID FIELD EXTINCTION MAPS; STAR-FORMATION; MILKY-WAY; CO SURVEY; NEBULAE;
CATALOG; YOUNG; GAS; DUST
AB We present an analysis of wide-field infrared extinction maps of a region in Perseus just north of the Taurus-Auriga dark cloud complex. From this analysis we have identified a massive, nearby, but previously unrecognized, giant molecular cloud (GMC). Both a uniform foreground star density and measurements of the cloud's velocity field from CO observations indicate that this cloud is likely a coherent structure at a single distance. From comparison of foreground star counts with Galactic models, we derive a distance of 450 +/- 23 pc to the cloud. At this distance the cloud extends over roughly 80 pc and has a mass of approximate to 10(5) M(circle dot), rivaling the Orion (A) molecular cloud as the largest and most massive GMC in the solar neighborhood. Although surprisingly similar in mass and size to the more famous Orion molecular cloud (OMC) the newly recognized cloud displays significantly less star formation activity with more than an order of magnitude fewer young stellar objects than found in the OMC, suggesting that both the level of star formation and perhaps the star formation rate in this cloud are an order of magnitude or more lower than in the OMC. Analysis of extinction maps of both clouds shows that the new cloud contains only 10% the amount of high extinction (A(K) > 1.0 mag) material as is found in the OMC. This, in turn, suggests that the level of star formation activity and perhaps the star formation rate in these two clouds may be directly proportional to the total amount of high extinction material and presumably high density gas within them and that there might be a density threshold for star formation on the order of n(H(2)) approximate to a few x 10(4) cm(-3).
C1 [Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lombardi, Marco] European So Observ, D-85748 Garching, Germany.
[Alves, Joao F.] Calar Alto Observ, Almeria 04004, Spain.
RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM clada@cfa.harvard.edu; mlombard@eso.org; jalves@caha.es
OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921
NR 33
TC 54
Z9 54
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 52
EP 59
DI 10.1088/0004-637X/703/1/52
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000006
ER
PT J
AU Brown, MJI
Moustakas, J
Caldwell, N
Palamara, D
Cool, RJ
Dey, A
Hickox, RC
Jannuzi, BT
Murray, SS
Zaritsky, D
AF Brown, Michael J. I.
Moustakas, John
Caldwell, Nelson
Palamara, David
Cool, Richard J.
Dey, Arjun
Hickox, Ryan C.
Jannuzi, Buell T.
Murray, Stephen S.
Zaritsky, Dennis
TI ACTIVE GALACTIC NUCLEI AND THE TRUNCATION OF STAR FORMATION IN K plus A
GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: individual (IRAS
14344+3451); galaxies: interactions; X-rays: galaxies
ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; RAY SOURCE CATALOG;
POSTSTARBURST GALAXIES; E+A-GALAXIES; LUMINOSITY FUNCTIONS; STARBURST
GALAXIES; PERSEUS CLUSTER; DISK GALAXIES; HOST GALAXIES
AB We have searched for active galactic nuclei (AGNs) in K+A galaxies, using multiwavelength imaging and spectroscopy in the Bootes field of the NOAO Deep Wide-Field Survey. The K+A galaxies, which have had their star formation rapidly truncated, are selected via their strong Balmer absorption lines and weak H alpha emission. Our sample consists of 24 K+A galaxies selected from 6594 0.10 < z < 0.35 galaxies brighter than I = 20 with optical spectroscopy from the AGN and Galaxy Evolution Survey. Two thirds of the K+A galaxies are likely ongoing galaxy mergers, with nearby companion galaxies or tidal tails. Galaxy mergers may be responsible for the truncation of star formation, or we are observing the aftermath of merger triggered starbursts. As expected, the optical colors of K+A galaxies largely fall between blue galaxies with ongoing star formation and red passive galaxies. However, only 1% of the galaxies with colors between the red and blue populations are K+A galaxies, and we conclude that the truncation of star formation in K+A galaxies must have been unusually abrupt (less than or similar to 100 Myr). We examined the AGN content of K+A galaxies with both optical emission-line ratios (BPT diagrams) and Chandra X-ray imaging. At least half of all K+A galaxies display the optical emission-line ratios of AGNs, and a third of M(R) < -22 K+A galaxies host AGNs with X-ray luminosities of similar to 10(42) erg s(-1). The faintest K+A galaxies do not show clear evidence for hosting AGNs, having emission-line ratios consistent with photoionization by massive stars and few X-ray detections. We speculate that two mechanisms may be responsible for the truncation of star formation in K+A galaxies, with AGN feedback only playing a role in M(R) less than or similar to -20.5 galaxies.
C1 [Brown, Michael J. I.; Palamara, David] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Moustakas, John] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Caldwell, Nelson] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Hickox, Ryan C.; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Brown, MJI (reprint author), Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
EM Michael.Brown@sci.monash.edu.au
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU NASA through Hubble Fellowship [HST-HF-01217.01]; Space Telescope
Science Institute; NASA [06-GALEX06-0030]; Spitzer [G05-AR-50443]; NOAO
FX We thank our colleagues on the AGES, NDWFS, and XBootes teams. This
paper would not have been possible without the efforts of the Chandra,
KPNO, and MMT support staff. David Palamara's involvement in this paper
began during his studies for Monash University's PHS3360 unit, which was
coordinated by John Cashion. Late in the development of this work,
Richard Cool was supported by NASA through Hubble Fellowship grant
HST-HF-01217.01, awarded by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, for NASA, under the contract NAS 5-26555. John Moustakas
received support from NASA grant 06-GALEX06-0030 and Spitzer grant
G05-AR-50443 during the development of this paper. Spectroscopic
observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
This work made use of optical images provided by NDWFS (Jannuzi & Dey
1999), which is supported by NOAO. NOAO is operated by AURA, Inc., under
a cooperative agreement with the National Science Foundation.
NR 64
TC 11
Z9 12
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 150
EP 158
DI 10.1088/0004-637X/703/1/150
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000017
ER
PT J
AU Acciari, VA
Aliu, E
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bradbury, SM
Buckley, JH
Bugaev, V
Butt, Y
Cannon, A
Celik, O
Cesarini, A
Chow, YC
Ciupik, L
Cogan, P
Colin, P
Cui, W
Dickherber, R
Duke, C
Falcone, AD
Fegan, SJ
Finley, JP
Finnegan, G
Fortin, P
Fortson, L
Furniss, A
Gall, D
Gillanders, GH
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Horan, D
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Kildea, J
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McCann, A
Millis, J
Moriarty, P
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Schroedter, M
Sembroski, GH
Smith, AW
Steele, D
Swordy, SP
Theiling, M
Toner, JA
Varlotta, A
Vincent, S
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wissel, S
Zitzer, B
Perez, ID
Ibarra, A
Anderhub, PRH
Antonelli, LA
Antoranz, P
Backes, M
Baixeras, C
Balestra, S
Barrio, JA
Bastieri, D
Gonzalez, JB
Becker, JK
Bednarek, W
Berger, K
Bernardini, E
Biland, A
Bock, RK
Bonnoli, G
Bordas, P
Tridon, DB
Bosch-Ramon, V
Bose, D
Braun, I
Bretz, T
Britvitch, I
Camara, M
Carmona, E
Carosi, A
Commichau, S
Contreras, JL
Cortina, J
Costado, MT
Covino, S
Curtef, V
Dazzi, F
De Angelis, A
Del Pozo, ED
Mendez, CD
De Los Reyes, R
De Lotto, B
De Maria, M
De Sabata, F
Dominguez, A
Dorner, D
Doro, M
Elsaesser, D
Errando, M
Ferenc, D
Fernandez, E
Firpo, R
Fonseca, MV
Font, L
Galante, N
Lopez, RJ
Garczarczyk, M
Gaug, M
Goebel, F
Hadasch, D
Hayashida, M
Herrero, A
Hildebrand, D
Hohne-Monch, D
Hose, J
Hsu, CC
Jogler, T
Kranich, D
La Barbera, A
Laille, A
Leonardo, E
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lorenz, E
Majumdar, P
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Mariotti, M
Martinez, M
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Miyamoto, H
Moldon, J
Moles, M
Moralejo, A
Nieto, D
Nilsson, K
Ninkovic, J
Orito, R
Oya, I
Paoletti, R
Paredes, JM
Pasanen, M
Pascoli, D
Pauss, F
Pegna, RG
Perez-Torres, MA
Persic, M
Peruzzo, L
Prada, F
Prandini, E
Puchades, N
Reichardt, I
Rhode, W
Ribo, M
Rico, J
Rissi, M
Robert, A
Rugamer, S
Saggion, A
Saito, TY
Salvati, M
Sanchez-Conde, M
Satalecka, K
Scalzotto, V
Scapin, V
Schweizer, T
Shayduk, M
Shore, SN
Sidro, N
Sierpowska-Bartosik, A
Silanpaa, A
Sitarek, J
Sobczynska, D
Spanier, F
Spiro, S
Stamerra, A
Stark, LS
Takalo, L
Tavecchio, F
Temnikov, P
Tescaro, D
Teshima, M
Tluczykont, M
Torres, DF
Turini, N
Vankov, H
Wagner, RM
Zabalza, V
Zandanel, F
Zanin, R
Zapatero, J
AF Acciari, V. A.
Aliu, E.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Butt, Y.
Cannon, A.
Celik, O.
Cesarini, A.
Chow, Y. C.
Ciupik, L.
Cogan, P.
Colin, P.
Cui, W.
Dickherber, R.
Duke, C.
Falcone, A. D.
Fegan, S. J.
Finley, J. P.
Finnegan, G.
Fortin, P.
Fortson, L.
Furniss, A.
Gall, D.
Gillanders, G. H.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Horan, D.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Kildea, J.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McCann, A.
Millis, J.
Moriarty, P.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Schroedter, M.
Sembroski, G. H.
Smith, A. W.
Steele, D.
Swordy, S. P.
Theiling, M.
Toner, J. A.
Varlotta, A.
Vincent, S.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wissel, S.
Zitzer, B.
de la Calle Perez, I.
Ibarra, A.
Anderhub, P. Rodriguez H.
Antonelli, L. A.
Antoranz, P.
Backes, M.
Baixeras, C.
Balestra, S.
Barrio, J. A.
Bastieri, D.
Becerra Gonzalez, J.
Becker, J. K.
Bednarek, W.
Berger, K.
Bernardini, E.
Biland, A.
Bock, R. K.
Bonnoli, G.
Bordas, P.
Tridon, D. Borla
Bosch-Ramon, V.
Bose, D.
Braun, I.
Bretz, T.
Britvitch, I.
Camara, M.
Carmona, E.
Carosi, A.
Commichau, S.
Contreras, J. L.
Cortina, J.
Costado, M. T.
Covino, S.
Curtef, V.
Dazzi, F.
De Angelis, A.
De Cea Del Pozo, E.
Delgado Mendez, C.
De Los Reyes, R.
De Lotto, B.
De Maria, M.
De Sabata, F.
Dominguez, A.
Dorner, D.
Doro, M.
Elsaesser, D.
Errando, M.
Ferenc, D.
Fernandez, E.
Firpo, R.
Fonseca, M. V.
Font, L.
Galante, N.
Garcia Lopez, R. J.
Garczarczyk, M.
Gaug, M.
Goebel, F.
Hadasch, D.
Hayashida, M.
Herrero, A.
Hildebrand, D.
Hoehne-Moench, D.
Hose, J.
Hsu, C. C.
Jogler, T.
Kranich, D.
La Barbera, A.
Laille, A.
Leonardo, E.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lorenz, E.
Majumdar, P.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Mariotti, M.
Martinez, M.
Mazin, D.
Meucci, M.
Miranda, J. M.
Mirzoyan, R.
Miyamoto, H.
Moldon, J.
Moles, M.
Moralejo, A.
Nieto, D.
Nilsson, K.
Ninkovic, J.
Orito, R.
Oya, I.
Paoletti, R.
Paredes, J. M.
Pasanen, M.
Pascoli, D.
Pauss, F.
Pegna, R. G.
Perez-Torres, M. A.
Persic, M.
Peruzzo, L.
Prada, F.
Prandini, E.
Puchades, N.
Reichardt, I.
Rhode, W.
Ribo, M.
Rico, J.
Rissi, M.
Robert, A.
Ruegamer, S.
Saggion, A.
Saito, T. Y.
Salvati, M.
Sanchez-Conde, M.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schweizer, T.
Shayduk, M.
Shore, S. N.
Sidro, N.
Sierpowska-Bartosik, A.
Silanpaa, A.
Sitarek, J.
Sobczynska, D.
Spanier, F.
Spiro, S.
Stamerra, A.
Stark, L. S.
Takalo, L.
Tavecchio, F.
Temnikov, P.
Tescaro, D.
Teshima, M.
Tluczykont, M.
Torres, D. F.
Turini, N.
Vankov, H.
Wagner, R. M.
Zabalza, V.
Zandanel, F.
Zanin, R.
Zapatero, J.
CA VERITAS Collaboration
MAGIC Collaboration
TI SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF MARKARIAN 421 DURING
OUTBURST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma
rays: observations; radiation mechanisms: non-thermal; X-rays: galaxies
ID ACTIVE GALAXY MARKARIAN-421; RAY SPECTRAL VARIABILITY; XMM-NEWTON;
CORRELATED VARIABILITY; MAGIC TELESCOPE; GALACTIC NUCLEI; TEV PHOTONS;
GAMMA-RAYS; ENERGY; RADIATION
AB We report on the results of two coordinated multiwavelength campaigns that focused on the blazar Markarian 421 during its 2006 and 2008 outbursts. These campaigns obtained UV and X-ray data using the XMM-Newton satellite, while the gamma-ray data were obtained utilizing three imaging atmospheric Cerenkov telescopes, the Whipple 10 m telescope and VERITAS, both based in Arizona, as well as the MAGIC telescope, based on La Palma in the Canary Islands. The coordinated effort between the gamma-ray groups allowed for truly simultaneous data in UV/X-ray/gamma-ray wavelengths during a significant portion of the XMM-Newton observations. This simultaneous coverage allowed for a reliable search for correlations between UV, X-ray, and gamma-ray variability over the course of the observations. Investigations of spectral hysteresis and modeling of the spectral energy distributions are also presented.
C1 [Acciari, V. A.; Benbow, W.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Finley, J. P.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Butt, Y.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Colin, P.; Finnegan, G.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fortin, P.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Horan, D.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France.
[Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[de la Calle Perez, I.; Ibarra, A.] ESA, European Space Astron Ctr, XMM Newton SOC, Madrid 28691, Spain.
[Anderhub, P. Rodriguez H.; Biland, A.; Braun, I.; Britvitch, I.; Commichau, S.; Dorner, D.; Hildebrand, D.; Kranich, D.; Lorenz, E.; Pauss, F.; Rissi, M.; Stark, L. S.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Antonelli, L. A.; Carosi, A.; Covino, S.; La Barbera, A.; Maraschi, L.; Salvati, M.; Spiro, S.; Tavecchio, F.] Natl Inst Astrophys, INAF, I-00136 Rome, Italy.
[Antoranz, P.; Balestra, S.; Barrio, J. A.; Bose, D.; Camara, M.; Contreras, J. L.; De Los Reyes, R.; Fonseca, M. V.; Miranda, J. M.; Nieto, D.; Oya, I.] Univ Complutense, E-28040 Madrid, Spain.
[Backes, M.; Becker, J. K.; Curtef, V.; Rhode, W.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Baixeras, C.; Font, L.; Hadasch, D.; Robert, A.; Zapatero, J.] Univ Autonoma Barcelona, E-08193 Barcelona, Spain.
[Bastieri, D.; Bock, R. K.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Pascoli, D.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.] Univ Padua, I-35131 Padua, Italy.
[Bastieri, D.; Bock, R. K.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Pascoli, D.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Becerra Gonzalez, J.; Costado, M. T.; Delgado Mendez, C.; Garcia Lopez, R. J.; Gaug, M.; Herrero, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Bednarek, W.; Berger, K.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; Majumdar, P.; Satalecka, K.; Tluczykont, M.] DESY, D-15738 Zeuthen, Germany.
[Bock, R. K.; Tridon, D. Borla; Carmona, E.; Galante, N.; Goebel, F.; Hayashida, M.; Hose, J.; Hsu, C. C.; Jogler, T.; Lorenz, E.; Mirzoyan, R.; Miyamoto, H.; Ninkovic, J.; Orito, R.; Saito, T. Y.; Schweizer, T.; Shayduk, M.; Sitarek, J.; Teshima, M.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Bonnoli, G.; Leonardo, E.; Meucci, M.; Paoletti, R.; Pegna, R. G.; Stamerra, A.; Turini, N.] Univ Siena, I-53100 Siena, Italy.
[Bonnoli, G.; Leonardo, E.; Meucci, M.; Paoletti, R.; Pegna, R. G.; Stamerra, A.; Turini, N.] INFN Pisa, I-53100 Siena, Italy.
[Bordas, P.; Bosch-Ramon, V.; Moldon, J.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona, IEEC, ICC, E-08028 Barcelona, Spain.
[Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Cortina, J.; Errando, M.; Fernandez, E.; Firpo, R.; Garczarczyk, M.; Martinez, M.; Mazin, D.; Moralejo, A.; Puchades, N.; Reichardt, I.; Rico, J.; Sidro, N.; Tescaro, D.; Zanin, R.] INAF, E-08193 Barcelona, Spain.
[Costado, M. T.; Garcia Lopez, R. J.; Herrero, A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] Univ Udine, I-33100 Udine, Italy.
[Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Persic, M.; Scapin, V.] INFN Trieste, I-33100 Udine, Italy.
[De Cea Del Pozo, E.; Sierpowska-Bartosik, A.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Dominguez, A.; Moles, M.; Perez-Torres, M. A.; Prada, F.; Sanchez-Conde, M.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Ferenc, D.; Laille, A.] Univ Calif Davis, Davis, CA 95616 USA.
[Lindfors, E.; Nilsson, K.; Pasanen, M.; Silanpaa, A.; Takalo, L.] Turku Univ, Tuorla Observ, FI-21500 Piikkio, Finland.
[Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Persic, M.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Persic, M.] Ist Nazl Fis Nucl, I-34143 Trieste, Italy.
[Rico, J.; Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy.
RP Cui, W (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
EM cui@physics.purdue.edu; dgall@physics.purdue.edu
RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Delgado,
Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Miranda, Jose
Miguel/F-2913-2013; Contreras Gonzalez, Jose Luis/K-7255-2014; Maneva,
Galina/L-7120-2016; Backes, Michael/N-5126-2016; Torres,
Diego/O-9422-2016; Reichardt, Ignasi/P-7478-2016; Temnikov,
Petar/L-6999-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017;
Braun, Isabel/C-9373-2012; Mannheim, Karl/F-6705-2012; Doro,
Michele/F-9458-2012; Tjus, Julia/G-8145-2012; Rico, Javier/K-8004-2014;
Fernandez, Ester/K-9734-2014; GAug, Markus/L-2340-2014; Lopez Moya,
Marcos/L-2304-2014; Font, Lluis/L-4197-2014; Fernandez,
Enrique/L-5387-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo,
Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015;
OI Spanier, Felix/0000-0001-6802-4744; Dominguez,
Alberto/0000-0002-3433-4610; Bastieri, Denis/0000-0002-6954-8862; Ribo,
Marc/0000-0002-9931-4557; Pandel, Dirk/0000-0003-2085-5586; Lang,
Mark/0000-0003-4641-4201; Covino, Stefano/0000-0001-9078-5507; Bordas,
Pol/0000-0002-0266-8536; Paredes, Josep M./0000-0002-1566-9044; Oya,
Igor/0000-0002-3881-9324; Turini, Nicola/0000-0002-9395-5230; Costado,
M. Teresa/0000-0002-2672-4061; LA BARBERA, ANTONINO/0000-0002-5880-8913;
Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610;
leonardo, elvira/0000-0003-0271-7673; de los Reyes Lopez,
Raquel/0000-0003-0485-9552; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480;
Hsu, Ching-Cheng/0000-0001-9406-2023; De Angelis,
Alessandro/0000-0002-3288-2517; Persic, Massimo/0000-0003-1853-4900;
Ward, John E/0000-0003-1973-0794; Delgado, Carlos/0000-0002-7014-4101;
Nieto, Daniel/0000-0003-3343-0755; Miranda, Jose
Miguel/0000-0002-1472-9690; Contreras Gonzalez, Jose
Luis/0000-0001-7282-2394; Backes, Michael/0000-0002-9326-6400; Torres,
Diego/0000-0002-1522-9065; Reichardt, Ignasi/0000-0003-3694-3820;
Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259;
Cortina, Juan/0000-0003-4576-0452; Bonnoli, Giacomo/0000-0003-2464-9077;
Mazin, Daniel/0000-0002-2010-4005; Stamerra,
Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Braun,
Isabel/0000-0002-9389-0502; Doro, Michele/0000-0001-9104-3214; Rico,
Javier/0000-0003-4137-1134; GAug, Markus/0000-0001-8442-7877; Lopez
Moya, Marcos/0000-0002-8791-7908; Font, Lluis/0000-0003-2109-5961;
Fernandez, Enrique/0000-0002-6405-9488; Moralejo Olaizola,
Abelardo/0000-0002-1344-9080; Antoranz, Pedro/0000-0002-3015-3601;
Becerra Gonzalez, Josefa/0000-0002-6729-9022
FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian
Institution; NSERC in Canada; Science Foundation Ireland; STFC, U.K;
NASA [NNX06AB96G, NNX08AD76G, NNX08AX53G]; ETH [TH 34/043]; Polish
MNiSzW [N N203 390834]; Helmholtz Gemeinschaft
FX The VERITAS research was supported by grants from the U.S. Department of
Energy, the U.S. National Science Foundation and the Smithsonian
Institution, by NSERC in Canada, by Science Foundation Ireland, and by
STFC in the U.K. We acknowledge the excellent work of the technical
support staff at the FLWO and the collaborating institutions in the
construction and operation of the instrument. D. G. and W. C. wish to
acknowledge support by NASA through grants NNX06AB96G, NNX08AD76G, and
NNX08AX53G. The MAGIC Collaboration thanks 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, and Spanish MCINN is gratefully acknowledged.
This work was also supported by ETH Research Grant TH 34/043, by the
Polish MNiSzW Grant N N203 390834, and by the YIP of the Helmholtz
Gemeinschaft. Facilities: MAGIC, VERITAS, FLWO:10m, XMM
NR 46
TC 31
Z9 31
U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 169
EP 178
DI 10.1088/0004-637X/703/1/169
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000019
ER
PT J
AU Drout, MR
Massey, P
Meynet, G
Tokarz, S
Caldwell, N
AF Drout, Maria R.
Massey, Philip
Meynet, Georges
Tokarz, Susan
Caldwell, Nelson
TI YELLOW SUPERGIANTS IN THE ANDROMEDA GALAXY (M31)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); galaxies: stellar content; stars: evolution;
supergiants
ID CURRENTLY FORMING STARS; INITIAL MASS FUNCTION; BVRI CCD PHOTOMETRY;
LOCAL GROUP; STELLAR EVOLUTION; RED SUPERGIANTS; NEARBY GALAXIES;
EFFECTIVE TEMPERATURES; UBVRI PHOTOMETRY; LUMINOUS STARS
AB The yellow supergiant content of nearby galaxies can provide a critical test of stellar evolution theory, bridging the gap between the hot, massive stars and the cool red supergiants. But, this region of the color-magnitude diagram is dominated by foreground contamination, requiring membership to somehow be determined. Fortunately, the large negative systemic velocity of M31, coupled to its high rotation rate, provides the means for separating the contaminating foreground dwarfs from the bona fide yellow supergiants within M31. We obtained radial velocities of similar to 2900 individual targets within the correct color-magnitude range corresponding to masses of 12 M(circle dot) and higher. A comparison of these velocities to those expected from M31's rotation curve reveals 54 rank-1 (near certain) and 66 rank-2 (probable) yellow supergiant members, indicating a foreground contamination >= 96%. We expect some modest contamination from Milky Way halo giants among the remainder, particularly for the rank-2 candidates, and indeed follow-up spectroscopy of a small sample eliminates four rank 2's while confirming five others. We find excellent agreement between the location of yellow supergiants in the H-R diagram and that predicted by the latest Geneva evolutionary tracks that include rotation. However, the relative number of yellow supergiants seen as a function of mass varies from that predicted by the models by a factor of > 10, in the sense that more high-mass yellow supergiants are predicted than those are actually observed. Comparing the total number (16) of > 20 M(circle dot) yellow supergiants with the estimated number (24,800) of unevolved O stars indicates that the duration of the yellow supergiant phase is similar to 3000 years. This is consistent with what the 12 M(circle dot) and 15 M(circle dot) evolutionary tracks predict, but disagrees with the 20,000-80,000 year timescales predicted by the models for higher masses.
C1 [Drout, Maria R.; Massey, Philip] Lowell Observ, Flagstaff, AZ 86001 USA.
[Meynet, Georges] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland.
[Tokarz, Susan; Caldwell, Nelson] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Drout, MR (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA.
EM maria-drout@uiowa.edu; Phil.Massey@lowell.edu; georges.meynet@unige.ch;
tokarz@cfa.harvard.edu; caldwell@cfa.harvard.edu
FU National Science Foundation [AST-0453611, AST-0604569]
FX We gratefully acknowledge the fine support at the MMT Observatory. M. R.
D.'s work was supported through a National Science Foundation REU grant,
AST-0453611, while P. M.'s efforts were supported through AST-0604569.
We are grateful to the Kitt Peak National Observatory Director, Buell
Jannuzi, and to Di Harmer for their efforts in obtaining the follow-up
spectra; Harmer and Brian Skiff also offered useful advice that aided in
our interpretation of these data. Knut Olsen made useful comments on the
recent star formation history of M31, and Heather Morrison provided
useful correspondence on the issue of foreground halo stars. We also
thank the anonymous referee for useful suggestions that improved the
paper.
NR 56
TC 36
Z9 36
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 441
EP 460
DI 10.1088/0004-637X/703/1/441
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000039
ER
PT J
AU Cerrigone, L
Hora, JL
Umana, G
Trigilio, C
AF Cerrigone, Luciano
Hora, Joseph L.
Umana, Grazia
Trigilio, Corrado
TI SPITZER DETECTION OF POLYCYCLIC AROMATIC HYDROCARBONS AND SILICATE
FEATURES IN POST-AGB STARS AND YOUNG PLANETARY NEBULAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: general; planetary nebulae: general; stars: AGB and post-AGB
ID ARRAY CAMERA IRAC; SPACE-TELESCOPE; EMISSION BANDS; INFRARED
SPECTROGRAPH; CIRCUMSTELLAR DUST; EVOLVED STARS; PAH EMISSION;
GRAIN-GROWTH; INTERSTELLAR; DISKS
AB We have observed a small sample of hot post-asymptotic giant branch (AGB) stars with the Infrared Array Camera (IRAC) and the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. The stars were selected from the literature on the basis of their far-infrared (IR) excess (i.e., post-AGB candidates) and B spectral type (i.e., close to the ionization of the envelope). The combination of our IRAC observations with Two Micron All Sky Survey and IRAS catalog data, along with previous radio observations in the cm range (where available) allowed us to model the spectral energy distributions of our targets and find that in almost all of them at least two shells of dust at different temperatures must be present, the hot dust component ranging up to 10(3) K. In several targets, grains larger than 1 mu m are needed to match the far-IR data points. In particular, in IRAS 17423-1755 grains up to 100 mu m must be introduced to match the emission in the millimeter range. We obtained IRS spectra to identify the chemistry of the envelopes and found that more than one-third of the sources in our sample have mixed chemistry, showing both mid-IR bands attributed to polycyclic aromatic hydrocarbons (PAHs) and silicate features. The analysis of the PAH features indicates that these molecules are located in the outflows, far away from the central stars. We consider the larger than expected percentage of mixed-chemistry targets as a selection bias toward stars with a disk or torus around them. Our results strengthen the current picture of mixed chemistry being due to the spatial segregation of different dust populations in the envelopes.
C1 [Cerrigone, Luciano] Max Planck Inst Radioastron, D-5300 Bonn, Germany.
[Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Umana, Grazia; Trigilio, Corrado] Catania Astrophys Observ, INAF, Catania, Italy.
RP Cerrigone, L (reprint author), Max Planck Inst Radioastron, Hugel 69, D-5300 Bonn, Germany.
OI Hora, Joseph/0000-0002-5599-4650
FU Smithsonian Astrophysical Observatory through the SAO Predoctoral
Program; NASA
FX L. Cerrigone acknowledges funding from the Smithsonian Astrophysical
Observatory through the SAO Predoctoral Program. 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. We would like
to thank an anonymous referee for his criticism, which led to a
substantial improvement of the paper.
NR 58
TC 31
Z9 31
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 585
EP 600
DI 10.1088/0004-637X/703/1/585
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000047
ER
PT J
AU Walborn, NR
Nichols, JS
Waldron, WL
AF Walborn, Nolan R.
Nichols, Joy S.
Waldron, Wayne L.
TI THE CORRELATION BETWEEN X-RAY LINE IONIZATION AND OPTICAL SPECTRAL TYPES
OF THE OB STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: early-type; stars: fundamental parameters; stars: winds,
outflows; X-rays: stars
ID XMM-NEWTON OBSERVATIONS; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; RESOLUTION
CHANDRA SPECTROSCOPY; SUPERGIANT ZETA-ORIONIS; SEQUENCE B-STARS;
EMISSION-LINES; STELLAR WINDS; HOT STARS; GAMMA-CASSIOPEIAE;
DELTA-ORIONIS
AB Marked correlations are reported between the ionization of the X-ray line spectra of normal OB stars, as observed by the Chandra X-Ray Observatory, and their optical spectral types. These correlations include the progressive weakening of the higher ionization relative to the lower ionization X-ray lines with advancing spectral type, and the similarly decreasing intensity ratios of the H-like to He-like lines of the a ions. These relationships were not predicted by models, nor have they been clearly evident in astrophysical studies of a few objects; rather, they have emerged from morphological analysis of an adequate ( albeit still small) sample, from which known peculiar objects such as magnetic stars and very rapid rotators have been isolated to reveal the normal trends. This process is analogous to that which first demonstrated the strong relationships between the UV wind profiles and the optical spectral types of normal OB stars, which likely bear a physical as well as a historical connection to the present X-ray results. Since the optical spectral types are calibrated in terms of fundamental stellar parameters, it follows that the winds and X-ray spectra are determined by the latter. These observations provide strong guidance for further astrophysical modeling of these phenomena.
C1 [Walborn, Nolan R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Nichols, Joy S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Waldron, Wayne L.] Eureka Sci Inc, Oakland, CA 94602 USA.
RP Walborn, NR (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM walborn@stsci.edu; jnichols@cfa.harvard.edu; wwaldron@satx.rr.com
NR 65
TC 17
Z9 17
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 633
EP 641
DI 10.1088/0004-637X/703/1/633
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000051
ER
PT J
AU Mao, SA
Psaltis, D
Milsom, JA
AF Mao, S. A.
Psaltis, Dimitrios
Milsom, John A.
TI SUPER-KEPLERIAN FREQUENCIES IN ACCRETION DISKS. IMPLICATIONS FOR MASS
AND SPIN MEASUREMENTS OF COMPACT OBJECTS FROM X-RAY VARIABILITY STUDIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; hydrodynamics
ID INERTIAL-ACOUSTIC OSCILLATIONS; GRO J1655-40; BLACK-HOLES; DISCS;
BINARIES
AB The detection of fast quasi-periodic variability from accreting black holes and neutron stars has been used to constrain their masses, radii, and spins. If the observed oscillations are linear modes in the accretion disks, then bounds can be placed on the properties of the central objects by assuming that these modes are locally sub-Keplerian. If, on the other hand, the observed oscillations correspond to nonlinear resonances between disk modes, then the properties of the central objects can be measured by assuming that the resonant modes are excited at the same radial annulus in the disk. In this paper, we use numerical simulations of vertically integrated, axisymmetric hydrodynamic accretion disks to provide examples of situations in which the assumptions implicit in both methods are not satisfied. We then discuss our results for the robustness of the mass and spin measurements of compact objects from variability studies.
C1 [Mao, S. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Psaltis, Dimitrios; Milsom, John A.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Psaltis, Dimitrios] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
RP Mao, SA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM samao@cfa.harvard.edu
FU NSF CAREER [NSF 0746549]
FX D. P. was supported in part by the NSF CAREER award NSF 0746549.
NR 16
TC 3
Z9 3
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 717
EP 720
DI 10.1088/0004-637X/703/1/717
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000058
ER
PT J
AU Lister, TA
Anderson, DR
Gillon, M
Hebb, L
Smalley, BS
Triaud, AHMJ
Cameron, AC
Wilson, DM
West, RG
Bentley, SJ
Christian, DJ
Enoch, R
Haswell, CA
Hellier, C
Horne, K
Irwin, J
Joshi, YC
Kane, SR
Mayor, M
Maxted, PFL
Norton, AJ
Parley, N
Pepe, F
Pollacco, D
Queloz, D
Ryans, R
Segransan, D
Skillen, I
Street, RA
Todd, I
Udry, S
Wheatley, PJ
AF Lister, T. A.
Anderson, D. R.
Gillon, M.
Hebb, L.
Smalley, B. S.
Triaud, A. H. M. J.
Cameron, A. Collier
Wilson, D. M.
West, R. G.
Bentley, S. J.
Christian, D. J.
Enoch, R.
Haswell, C. A.
Hellier, C.
Horne, K.
Irwin, J.
Joshi, Y. C.
Kane, S. R.
Mayor, M.
Maxted, P. F. L.
Norton, A. J.
Parley, N.
Pepe, F.
Pollacco, D.
Queloz, D.
Ryans, R.
Segransan, D.
Skillen, I.
Street, R. A.
Todd, I.
Udry, S.
Wheatley, P. J.
TI WASP-16b: A NEW JUPITER-LIKE PLANET TRANSITING A SOUTHERN SOLAR ANALOG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: abundances; stars: individual (WASP-16b)
ID MASS STARS; TELESCOPE; SUPERWASP; CANDIDATES; PHOTOMETRY; PROJECT;
SEARCH; MODELS
AB We report the discovery from WASP-South of a new Jupiter-like extrasolar planet, WASP-16b, which transits its solar analog host star every 3.12 days. Analysis of the transit photometry and radial velocity spectroscopic data leads to a planet with R(p) = 1.008 +/- 0.071 R(Jup) and M(p) = 0.855 +/- 0.059 M(Jup), orbiting a host star with R(*) = 0.946 +/- 0.054 R(circle dot) and M(*) = 1.022 +/- 0.101M(circle dot). Comparison of the high resolution stellar spectrum with synthetic spectra and stellar evolution models indicates the host star is a near-solar metallicity ([Fe/H] = 0.01 +/- 0.10) solar analog (T(eff) = 5700 +/- 150 K and log g = 4.5 +/- 0.2) of intermediate age (tau = 2.3(-2.2)(+5.8) Gyr).
C1 [Lister, T. A.; Street, R. A.] Las Cumbres Observ, Goleta, CA 93117 USA.
[Anderson, D. R.; Smalley, B. S.; Wilson, D. M.; Bentley, S. J.; Hellier, C.; Maxted, P. F. L.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Gillon, M.; Triaud, A. H. M. J.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Gillon, M.] Univ Liege, Inst Astrophys & Geophys, Liege 1, Belgium.
[Hebb, L.; Cameron, A. Collier; Enoch, R.; Horne, K.; Parley, N.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Wilson, D. M.] Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England.
[West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Christian, D. J.; Joshi, Y. C.; Pollacco, D.; Ryans, R.; Todd, I.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Christian, D. J.] Calif State Univ Northridge, Northridge, CA 91330 USA.
[Enoch, R.; Haswell, C. A.; Norton, A. J.; Parley, N.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kane, S. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Skillen, I.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain.
[Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
RP Lister, TA (reprint author), Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
EM tlister@lcogt.net
RI Kane, Stephen/B-4798-2013;
OI Norton, Andrew/0000-0001-7619-8269; Cameron, Andrew/0000-0002-8863-7828;
Triaud, Amaury/0000-0002-5510-8751; Christian,
Damian/0000-0003-1746-3020; Wheatley, Peter/0000-0003-1452-2240
FU South African Astronomical Observatory; consortium universities; UK's
Science and Technology Facilities Council
FX The WASP Consortium comprises the Universities of Keele, Leicester, St.
Andrews, the Queen's University Belfast, the Open University, and the
Isaac Newton Group. WASP-South is hosted by the South African
Astronomical Observatory, and we are grateful for their support and
assistance. Funding for WASP comes from the consortium universities and
from the UK's Science and Technology Facilities Council.
NR 22
TC 22
Z9 22
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 752
EP 756
DI 10.1088/0004-637X/703/1/752
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000061
ER
PT J
AU Knutson, HA
Charbonneau, D
Cowan, NB
Fortney, JJ
Showman, AP
Agol, E
Henry, GW
AF Knutson, Heather A.
Charbonneau, David
Cowan, Nicolas B.
Fortney, Jonathan J.
Showman, Adam P.
Agol, Eric
Henry, Gregory W.
TI THE 8 mu m PHASE VARIATION OF THE HOT SATURN HD 149026b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (HD 149026b); techniques:
photometric
ID INFRARED-EMISSION SPECTRUM; EXTRASOLAR GIANT PLANETS;
SPITZER-SPACE-TELESCOPE; LIGHT-CURVE PROJECT; ATMOSPHERIC CIRCULATION;
TEMPERATURE INVERSION; TRANSIT PHOTOMETRY; THERMAL EMISSION; ROTATION
PERIOD; JUPITERS
AB We monitor the star HD 149026 and its Saturn-mass planet at 8.0 mu m over slightly more than half an orbit using the Infrared Array Camera on the Spitzer Space Telescope. We find an increase of 0.0227% +/- 0.0066% (3.4 sigma significance) in the combined planet-star flux during this interval. The minimum flux from the planet is 45% +/- 19% of the maximum planet flux, corresponding to a difference in brightness temperature of 480 +/- 140 K between the two hemispheres. We derive a new secondary eclipse depth of 0.0411% +/- 0.0076% in this band, corresponding to a dayside brightness temperature of 1440 +/- 150 K. Our new secondary eclipse depth is half that of a previous measurement (3.0 sigma difference) in this same bandpass by Harrrington et al. We re-fit the Harrrington et al. data and obtain a comparably good fit with a smaller eclipse depth that is consistent with our new value. In contrast to earlier claims, our new eclipse depth suggests that this planet's dayside emission spectrum is relatively cool, with an 8 mu m brightness temperature that is less than the maximum planet-wide equilibrium temperature. We measure the interval between the transit and secondary eclipse and find that that the secondary eclipse occurs 20.9(-6.5)(+7.2) minutes earlier (2.9 sigma) than predicted for a circular orbit, a marginally significant result. This corresponds to e cos (omega) = -0.0079(-0.0025)(+0.0027), where e is the planet's orbital eccentricity and omega is the argument of pericenter.
C1 [Knutson, Heather A.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cowan, Nicolas B.; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
RP Knutson, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hknutson@cfa.harvard.edu
RI Agol, Eric/B-8775-2013
OI Agol, Eric/0000-0002-0802-9145
FU NASA; National Science Foundation
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract to NASA. Support for
this work was provided by NASA through an award issued by JPL/Caltech.
H. A. K. was supported by a National Science Foundation Graduate
Research Fellowship.
NR 75
TC 70
Z9 72
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 769
EP 784
DI 10.1088/0004-637X/703/1/769
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000063
ER
PT J
AU Kim, DW
Fabbiano, G
Brassington, NJ
Fragos, T
Kalogera, V
Zezas, A
Jordan, A
Sivakoff, GR
Kundu, A
Zepf, SE
Angelini, L
Davies, RL
Gallagher, JS
Juett, AM
King, AR
Pellegrini, S
Sarazin, CL
Trinchieri, G
AF Kim, D. -W.
Fabbiano, G.
Brassington, N. J.
Fragos, T.
Kalogera, V.
Zezas, A.
Jordan, A.
Sivakoff, G. R.
Kundu, A.
Zepf, S. E.
Angelini, L.
Davies, R. L.
Gallagher, J. S.
Juett, A. M.
King, A. R.
Pellegrini, S.
Sarazin, C. L.
Trinchieri, G.
TI COMPARING GC AND FIELD LMXBs IN ELLIPTICAL GALAXIES WITH DEEP CHANDRA
AND HUBBLE DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 3379,
NGC 4278, NGC 4697); X-rays: binaries; X-rays: galaxies
ID X-RAY BINARIES; GLOBULAR-CLUSTER CONNECTION; MULTIWAVELENGTH PROJECT;
LUMINOSITY FUNCTION; BLACK-HOLE; ULTRACOMPACT BINARIES; SOURCE CATALOG;
POINT SOURCES; CENTAURUS-A; NGC 3379
AB We present a statistical study of the low-mass X-ray binary (LMXB) populations of three nearby, old elliptical galaxies: NGC 3379, NGC 4278, and NGC 4697. With a cumulative similar to 1 Ms Chandra ACIS observing time, we detect 90-170 LMXBs within the D(25) ellipse of each galaxy. Cross-correlating Chandra X-ray sources and HST optical sources, we identify 75 globular cluster (GC) LMXBs and 112 field LMXBs with L(X) > 10(36) erg s(-1) ( detections of these populations are 90% complete down to luminosities in the range of 6 x 10(36) to 1.5 x 10(37) erg s(-1)). At the higher luminosities explored in previous studies, the statistics of this sample are consistent with the properties of GC-LMXBs reported in the literature. In the low-luminosity range allowed by our deeper data (L(X) < 5 x 10(37) erg s(-1)), we find a significant relative lack of GC-LMXBs, when compared with field sources. Using the co-added sample from the three galaxies, we find that the incompleteness-corrected X-ray luminosity functions (XLFs) of GC and field LMXBs differ at similar to 4 sigma significance at L(X) < 5 x 10(37) erg s(-1). As previously reported, these XLFs are consistent at higher luminosities. The presently available theoretical models for LMXB formation and evolution in clusters are not sophisticated enough to provide a definite explanation for the shape of the observed GC-LMXB XLF. Our observations may indicate a potential predominance of GC-LMXBs with donors evolved beyond the main sequence, when compared to current models, but their efficient formation requires relatively high initial binary fractions in clusters. The field LMXB XLF can be fitted with either a single power-law model plus a localized excess at a luminosity of (5-6) x 10(37) erg s(-1), or a broken power law with a similar low-luminosity break. This XLF may be explained with NS-red-giant LMXBs, contributing to similar to 15% of total LMXBs population at similar to 5 x 10(37) erg s(-1). The difference in the GC and field XLFs is consistent with different origins and/or evolutionary paths between the two LMXB populations, although a fraction of the field sources are likely to have originated in GCs.
C1 [Kim, D. -W.; Fabbiano, G.; Brassington, N. J.; Zezas, A.; Jordan, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fragos, T.; Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Kundu, A.; Zepf, S. E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Angelini, L.; Juett, A. M.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Davies, R. L.] Univ Oxford, Oxford, England.
[Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[King, A. R.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Trinchieri, G.] Osserv Astron Brera, INAF, I-20121 Milan, Italy.
RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM kim@cfa.harvard.edu; gfabbiano@cfa.harvard.edu; vicky@northwestern.edu;
azezas@cfa.harvard.edu; ajordan@astro.puc.cl; grs8g@virginia.edu;
zepf@pa.msu.edu; angelini@davide.gsfc.nasa.gov; rld@astro.ox.ac.uk;
jsg@astro.wisc.edu; Adrienne.M.Juett@nasa.gov; ark@star.le.ac.uk;
silvia.pellegrini@unibo.it; cls7i@virginia.edu;
ginevra.trinchieri@brera.inaf.it
RI Sivakoff, Gregory/G-9602-2011; Zezas, Andreas/C-7543-2011; Fragos,
Tassos/A-3581-2016;
OI Sivakoff, Gregory/0000-0001-6682-916X; Zezas,
Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X;
Fragos, Tassos/0000-0003-1474-1523; Jordan, Andres/0000-0002-5389-3944
FU CXC CIAO; CALDB; Chandra GO [G06-7079A, G06-7079B, GO7-8078X, GO7-8089A,
GO8-9085X]; NASA [NAS8-03060, NAG5-13056]; Northwestern University;
Hubble [HST-GO-10597.03-A, HST-GO-10582.02-A, HST-GO-10835.01-A]; Kavli
Institute for Theoretical Physics; National Science Foundation
[PHY05-51164]
FX We thank Chris Deloye, Natalia Ivanova, and Fred Rasio for very useful
discussions. The data analysis was supported by the CXC CIAO software
and CALDB. We have used the NASA NED and ADS facilities, and have
extracted archival data from the Chandra archives. This work was
supported by the Chandra GO grant G06-7079A ( PI: Fabbiano) and
subcontract G06-7079B ( PI: Kalogera). We acknowledge partial support
from NASA contract NAS8-03060 ( CXC). D.-W.K. acknowledges support from
Chandra archival research grant AR6-7008X, and A.Z. from NASA LTSA grant
NAG5-13056. T. F. acknowledges support by a Northwestern University
Presidential Fellowship. G. S., C. S., and A.J. were supported in part
by Hubble grants HST-GO-10597.03-A, HST-GO-10582.02-A, and
HST-GO-10835.01-A, and Chandra grants GO7-8078X, GO7-8089A, and
GO8-9085X. G. F., T. F., and V. K. also acknowledge support by the Kavli
Institute for Theoretical Physics at UCSB where part of this work was
completed. This research was supported in part by the National Science
Foundation under Grant PHY05-51164.
NR 74
TC 45
Z9 45
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 829
EP 844
DI 10.1088/0004-637X/703/1/829
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000067
ER
PT J
AU Pavlov, GG
Luna, GJM
AF Pavlov, G. G.
Luna, G. J. M.
TI A DEDICATED CHANDRA ACIS OBSERVATION OF THE CENTRAL COMPACT OBJECT IN
THE CASSIOPEIA A SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: neutron; supernovae: individual (Cassiopeia A)
ID X-RAY PULSAR; RESONANT CYCLOTRON SCATTERING; ISOLATED NEUTRON-STAR; A
SUPERNOVA; SPATIAL-RESOLUTION; MAGNETIC-FIELDS; INFRARED ECHOES;
POINT-SOURCE; CAS-A; DISCOVERY
AB We present results of a recent Chandra X-ray Observatory observation of the central compact object (CCO) in the supernova remnant (SNR) Cassiopeia A. This observation was carried out in an instrumental configuration that combines a high spatial resolution with a minimum spectral distortion, and it allowed us to search for pulsations with periods longer than approximate to 0.68 s. We found no evidence of extended emission associated with the CCO, nor statistically significant pulsations ( the 3 sigma upper limit on pulsed fraction is about 16%). The fits of the CCO spectrum with the power-law model yield a large photon index, Gamma approximate to 5, and a hydrogen column density larger than that obtained from the SNR spectra. The fits with the blackbody model are statistically unacceptable. Better fits are provided by hydrogen neutron star atmosphere models, with the best-fit effective temperature kT(eff)(infinity) approximate to 0.2 keV, but they require a small star's radius, R = 4-5.5 km, and a low mass, M less than or similar to 0.8M(circle dot). A neutron star cannot have so small radius and mass, but the observed emission might emerge from an atmosphere of a strange quark star. More likely, the CCO could be a neutron star with a nonuniform surface temperature and a low surface magnetic field ( the so-called anti-magnetar), similar to three other CCOs for which upper limits on period derivative have been established. The bolometric luminosity, L(bol)(infinity) similar to 6 x 10(33) erg s(-1), estimated from the fits with the hydrogen atmosphere models is consistent with the standard neutron star cooling for the CCO age of 330 yr. The origin of the surface temperature's nonuniformity remains to be understood; it might be caused by anisotropic heat conduction in the neutron star crust with very strong toroidal magnetic fields.
C1 [Pavlov, G. G.] Penn State Univ, University Pk, PA 16802 USA.
[Luna, G. J. M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Pavlov, GG (reprint author), Penn State Univ, 525 Davey Lab, University Pk, PA 16802 USA.
EM pavlov@astro.psu.edu; gluna@cfa.harvard.edu
FU National Aeronautics and Space Administration [GO6-7055X, NAS8-03060,
NNX09AC84G]
FX We thank Slava Zavlin for calculating nsagrav models for a broader
parameter domain, Dany Page for providing the NS and SQS M( R) relations
for various equations of state, Leisa Townsley for the discussions of
the CTI effects in ACIS, Nanda Rea for the discussion of the RCS
spectral model, Sandro Mereghetti for the discussion of the XMM-Newton
observation of Cas A, and Oleg Kargaltsev, Zdenka Misanovic and Bill
Joye for their useful advice on the data analysis. Support for this work
was provided by the National Aeronautics and Space Administration
through Chandra Award Number GO6-7055X 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. The work was also partially
supported by NASA grant NNX09AC84G.
NR 49
TC 31
Z9 31
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 910
EP 921
DI 10.1088/0004-637X/703/1/910
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000074
ER
PT J
AU Giodini, S
Pierini, D
Finoguenov, A
Pratt, GW
Boehringer, H
Leauthaud, A
Guzzo, L
Aussel, H
Bolzonella, M
Capak, P
Elvis, M
Hasinger, G
Ilbert, O
Kartaltepe, JS
Koekemoer, AM
Lilly, SJ
Massey, R
McCracken, HJ
Rhodes, J
Salvato, M
Sanders, DB
Scoville, NZ
Sasaki, S
Smolcic, V
Taniguchi, Y
Thompson, D
AF Giodini, S.
Pierini, D.
Finoguenov, A.
Pratt, G. W.
Boehringer, H.
Leauthaud, A.
Guzzo, L.
Aussel, H.
Bolzonella, M.
Capak, P.
Elvis, M.
Hasinger, G.
Ilbert, O.
Kartaltepe, J. S.
Koekemoer, A. M.
Lilly, S. J.
Massey, R.
McCracken, H. J.
Rhodes, J.
Salvato, M.
Sanders, D. B.
Scoville, N. Z.
Sasaki, S.
Smolcic, V.
Taniguchi, Y.
Thompson, D.
CA COSMOS Collaboration
TI STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE
REDSHIFT 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; cosmology: observations; diffuse radiation;
galaxies: clusters: general; galaxies: stellar content; X-rays:
galaxies: clusters
ID EVOLUTION SURVEY COSMOS; NEARBY GALAXY CLUSTERS; X-RAY LUMINOSITY;
DIFFUSE OPTICAL LIGHT; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; COLD
DARK-MATTER; M-T RELATION; STAR-FORMATION; XMM-NEWTON
AB We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 <= z <= 1 are selected from the COSMOS 2 deg(2) survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R(500). The total sample of 118 groups and clusters with z <= 1 spans a range in M(500) of similar to 10(13)-10(15) M(circle dot). We find that the stellar mass fraction associated with galaxies at R(500) decreases with increasing total mass as M(500)(-0.37+/-0.04), independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f(500)(stars+gas) = f(500)(stars) + f(500)(gas)) is found to increase by similar to 25%, when M(500) increases from < M > = 5 x 10(13) M(circle dot) to < M > = 7 x 10(14)M(circle dot). After consideration of a plausible contribution due to intracluster light (11%-22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3 sigma for groups of < M > = 5 x 10(13) M(circle dot). The discrepancy decreases toward higher total masses, such that it is 1 sigma at < M > = 7 x 10(14) M(circle dot). We discuss this result in terms of nongravitational processes such as feedback and filamentary heating.
C1 [Giodini, S.; Pierini, D.; Finoguenov, A.; Pratt, G. W.; Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Finoguenov, A.] Univ Maryland, Baltimore, MD 21250 USA.
[Leauthaud, A.] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA.
[Leauthaud, A.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Guzzo, L.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Aussel, H.] Univ Paris 07, AIM Unite Mixte Rech, CEA, CNRS,UMR N158, Paris, France.
[Bolzonella, M.] INAF, Bologna Astron Observ, I-40127 Bologna, Italy.
[Capak, P.; Scoville, N. Z.] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Capak, P.; Massey, R.; Rhodes, J.; Salvato, M.; Smolcic, V.; Thompson, D.] CALTECH, Pasadena, CA 91125 USA.
[Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hasinger, G.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Ilbert, O.; Kartaltepe, J. S.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lilly, S. J.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[McCracken, H. J.] Univ Paris 06, Inst Astrophys, UMR 7095, CNRS, F-75014 Paris, France.
[Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sasaki, S.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Sasaki, S.] Ehime Univ, Dept Phys, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan.
[Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
RP Giodini, S (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
RI Bolzonella, Micol/O-9495-2015;
OI Bolzonella, Micol/0000-0003-3278-4607; Koekemoer,
Anton/0000-0002-6610-2048
NR 84
TC 177
Z9 177
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 982
EP 993
DI 10.1088/0004-637X/703/1/982
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000081
ER
PT J
AU Zhu, C
Krems, R
Dalgarno, A
Balakrishnan, N
AF Zhu, C.
Krems, R.
Dalgarno, A.
Balakrishnan, N.
TI CHEMISTRY OF HYDROGEN FLUORIDE IN THE INTERSTELLAR MEDIUM (vol 577, pg
795, 2002)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Zhu, C.; Krems, R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Balakrishnan, N.] Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
RP Zhu, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 1
TC 0
Z9 0
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP
PY 2009
VL 703
IS 1
BP 1176
EP 1176
DI 10.1088/0004-637X/703/1/1176
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AE
UT WOS:000269625000098
ER
PT J
AU Modjaz, M
Li, W
Butler, N
Chornock, R
Perley, D
Blondin, S
Bloom, JS
Filippenko, AV
Kirshner, RP
Kocevski, D
Poznanski, D
Hicken, M
Foley, RJ
Stringfellow, GS
Berlind, P
Navascues, DBY
Blake, CH
Bouy, H
Brown, WR
Challis, P
Chen, H
de Vries, WH
Dufour, P
Falco, E
Friedman, A
Ganeshalingam, M
Garnavich, P
Holden, B
Illingworth, G
Lee, N
Liebert, J
Marion, GH
Olivier, SS
Prochaska, JX
Silverman, JM
Smith, N
Starr, D
Steele, TN
Stockton, A
Williams, GG
Wood-Vasey, WM
AF Modjaz, M.
Li, W.
Butler, N.
Chornock, R.
Perley, D.
Blondin, S.
Bloom, J. S.
Filippenko, A. V.
Kirshner, R. P.
Kocevski, D.
Poznanski, D.
Hicken, M.
Foley, R. J.
Stringfellow, G. S.
Berlind, P.
Barrado y Navascues, D.
Blake, C. H.
Bouy, H.
Brown, W. R.
Challis, P.
Chen, H.
de Vries, W. H.
Dufour, P.
Falco, E.
Friedman, A.
Ganeshalingam, M.
Garnavich, P.
Holden, B.
Illingworth, G.
Lee, N.
Liebert, J.
Marion, G. H.
Olivier, S. S.
Prochaska, J. X.
Silverman, J. M.
Smith, N.
Starr, D.
Steele, T. N.
Stockton, A.
Williams, G. G.
Wood-Vasey, W. M.
TI FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC
OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY
TRANSIENT 080109
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies: distances and redshifts; galaxies: individual (NGC 2770);
supernovae: general; supernovae: individual (SN 2008D)
ID CORE-COLLAPSE SUPERNOVA; NEUTRON-STAR KICKS; LIGHT CURVES; IA
SUPERNOVAE; IC SUPERNOVAE; MASSIVE STARS; OPTICAL SPECTROSCOPY; IMAGE
SUBTRACTION; UBVRI PHOTOMETRY; BURST CONNECTION
AB We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr before the detection of the X-ray transient to 150 days after its detection, and a detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines) and showed that SN 2008D had a relatively long rise time of 18 days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Delta t approximate to 0.1-4 days, most pronounced in the blue bands) followed by (56)Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E(K) and M(ej) from the literature, estimate the stellar radius R(star) of its probable Wolf-Rayet progenitor. According to the model of Waxman et al. and Chevalier & Fransson, we derive R(star)(W07) = 1.2 +/- 0.7 R(circle dot) and R(star)(CF08) = 12 +/- 7 R(circle dot), respectively; the latter being more in line with typical WN stars. Spectra obtained at three and four months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.
C1 [Modjaz, M.; Li, W.; Butler, N.; Chornock, R.; Perley, D.; Bloom, J. S.; Filippenko, A. V.; Kocevski, D.; Poznanski, D.; Foley, R. J.; Bouy, H.; Ganeshalingam, M.; Lee, N.; Silverman, J. M.; Smith, N.; Starr, D.; Steele, T. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Blondin, S.] ESO, D-85748 Garching, Germany.
[Blondin, S.; Kirshner, R. P.; Hicken, M.; Foley, R. J.; Berlind, P.; Blake, C. H.; Brown, W. R.; Challis, P.; Falco, E.; Friedman, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bloom, J. S.; Starr, D.] Las Cumbres Global Telescope Network, Santa Barbara, CA 93117 USA.
[Stringfellow, G. S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Barrado y Navascues, D.] CSIC, INTA, Ctr Astrobiol, LAEX, E-28691 Madrid, Spain.
[Bouy, H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Chen, H.] Univ Chicago, Dept Astron, Chicago, IL 60637 USA.
[de Vries, W. H.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[de Vries, W. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Dufour, P.; Liebert, J.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Holden, B.; Illingworth, G.; Prochaska, J. X.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Olivier, S. S.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Stockton, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Williams, G. G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
RP Modjaz, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM mmodjaz@astro.berkeley.edu
RI Friedman, Andrew/I-4691-2013; Barrado Navascues, David/C-1439-2017;
OI Friedman, Andrew/0000-0003-1334-039X; Barrado Navascues,
David/0000-0002-5971-9242; Bouy, Herve/0000-0002-7084-487X
NR 180
TC 115
Z9 118
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2009
VL 702
IS 1
BP 226
EP 248
DI 10.1088/0004-637X/702/1/226
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BD
UT WOS:000269244500016
ER
PT J
AU Salvesen, G
Raymond, JC
Edgar, RJ
AF Salvesen, Greg
Raymond, John C.
Edgar, Richard J.
TI SHOCK SPEED, COSMIC RAY PRESSURE, AND GAS TEMPERATURE IN THE CYGNUS LOOP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; ISM: individual (Cygnus Loop); shock waves; supernova
remnants
ID BALMER-DOMINATED SHOCKS; FORMED DENSE SHELL; SUPERNOVA-REMNANT; X-RAY;
NONRADIATIVE SHOCK; ASTROPHYSICAL SHOCKS; THERMAL CONDUCTION;
NORTHEASTERN RIM; MODELING W44; HOT INTERIOR
AB Upper limits on the shock speeds in supernova remnants can be combined with post-shock temperatures to obtain upper limits on the ratio of cosmic ray to gas pressure (P-CR/P-G) behind the shocks. We constrain shock speeds from proper motions and distance estimates, and we derive temperatures from X-ray spectra. The shock waves are observed as faint H alpha filaments stretching around the Cygnus Loop supernova remnant in two epochs of the Palomar Observatory Sky Survey (POSS) separated by 39.1 years. We measured proper motions of 18 nonradiative filaments and derived shock velocity limits based on a limit to the Cygnus Loop distance of 576 +/- 61 pc given by Blair et al. for a background star. The Position Sensitive Proportional Counter (PSPC) instrument on-board ROSAT observed the X-ray emission of the post-shock gas along the perimeter of the Cygnus Loop, and we measure post-shock electron temperature from spectral fits. Proper motions range from 2.'' 7 to 5.'' 4 over the POSS epochs and post-shock temperatures range from kT similar to 100-200 eV. Our analysis suggests a cosmic ray to post-shock gas pressure consistent with zero, and in some positions P-CR is formally smaller than zero. We conclude that the distance to the Cygnus Loop is close to the upper limit given by the distance to the background star and that either the electron temperatures are lower than those measured from ROSAT PSPC X-ray spectral fits or an additional heat input for the electrons, possibly due to thermal conduction, is required.
C1 [Salvesen, Greg; Raymond, John C.; Edgar, Richard J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Salvesen, Greg] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Salvesen, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM salvesen@head.cfa.harvard.edu; jraymond@cfa.harvard.edu;
edgar@head.cfa.harvard.edu
FU National Science Foundation Research Experiences for Undergraduates
(REU); Department of Defense Awards; Undergraduate Research Experiences
(ASSURE) [0754568]; Smithsonian Institution; NASA [NAS8-03060]
FX This work is supported in part by the National Science Foundation
Research Experiences for Undergraduates (REU) and Department of Defense
Awards to Stimulate and Support Undergraduate Research Experiences
(ASSURE) programs under grant 0754568 and by the Smithsonian
Institution.; We acknowledge generous data policies of the Space
Telescope Science Institute, for digitizing and archiving the Palomar
Observatory Sky Surveys, and the High Energy Astrophysics Space
Astronomy Archival Research Center (HEASARC) at the NASA/Goddard Space
Flight Center, for making the ROSAT data available. The Digitized Sky
Survey was produced at the Space Telescope Science Institute under US
Government grant NAG W-2166. The images of these surveys are based on
photographic data obtained using the Oschin Schmidt Telescope on Palomar
Mountain and the UK Schmidt Telescope. The plates were processed into
the present compressed digital form with the permission of these
institutions. R.J.E. acknowledges support from NASA contract NAS8-03060
(the Chandra X-ray Center) to the Smithsonian Astrophysical Observatory.
NR 52
TC 16
Z9 16
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2009
VL 702
IS 1
BP 327
EP 339
DI 10.1088/0004-637X/702/1/327
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BD
UT WOS:000269244500025
ER
PT J
AU Young, CH
Bourke, TL
Dunham, MM
Evans, NJ
Jorgensen, JK
Shirley, YL
Young, KE
De Vries, C
Claussen, MJ
Popa, V
AF Young, Chadwick H.
Bourke, Tyler L.
Dunham, Michael M.
Evans, Neal J., II
Jorgensen, Jes K.
Shirley, Yancy L.
Young, Kaisa E.
De Vries, Christopher
Claussen, Mark J.
Popa, Victor
TI THE SPITZER c2d SURVEY OF NEARBY DENSE CORES. VI. THE PROTOSTARS OF
LYNDS DARK NEBULA 1221
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual (L1221); ISM: jets and outflows; stars: formation;
stars: low-mass, brown dwarfs
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; RADIO-CONTINUUM
EMISSION; MASS STAR-FORMATION; T-TAURI STARS; SPACE-TELESCOPE; MOLECULAR
CLOUDS; PROTOSTELLAR SYSTEM; OUTFLOW SOURCES; IMAGING SURVEY
AB Observations of Lynds Dark Nebula 1221 from the Spitzer Space Telescope are presented. These data show three candidate protostars toward L1221, only two of which were previously known. The infrared observations also show signatures of outflowing material, an interpretation which is also supported by radio observations with the Very Large Array. In addition, molecular line maps from the Five College Radio Astronomy Observatory are shown. One-dimensional dust continuum modeling of two of these protostars, IRS1 and IRS3, is described. These models show two distinctly different protostars forming in very similar environments. IRS1 shows a higher luminosity and a larger inner radius of the envelope than IRS3. The disparity could be caused by a difference in age or mass, orientation of outflow cavities, or the impact of a binary in the IRS1 core.
C1 [Young, Chadwick H.; Young, Kaisa E.; Popa, Victor] Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA.
[Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dunham, Michael M.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-5300 Bonn, Germany.
[Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[De Vries, Christopher] Calif State Univ Stanislaus, Dept Phys Phys Sci & Geol, Turlock, CA 95382 USA.
[Claussen, Mark J.] NRAO, Socorro, NM 87801 USA.
RP Young, CH (reprint author), Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA.
RI Jorgensen, Jes Kristian/L-7936-2014
OI Jorgensen, Jes Kristian/0000-0001-9133-8047
FU NASA [1224608, 1279198, NAG5-10488, NNX07AJ72G, NGT5-50401, NGT5-40115]
FX Support for this work, part of the Spitzer Legacy Science Program, was
provided by NASA through contract 1224608 issued by the Jet Propulsion
Laboratory, California Institute of Technology, under NASA contract
1407, and the Smithsonian Astrophysical Observatory, under NASA contract
1279198. This work was also supported by NASA grants NAG5-10488 and
NNX07AJ72G. K. E. Y. was supported by NASA under Grant No. NGT5-50401
issued through the Office of Space Science. C. H. Y. thanks the
Louisiana Board of Regents, BoRSF, under agreement NASA/LEQSF
(2001-2005)-LaSPACE and NASA/LaSPACE under grant NGT5-40115 for support
during this project.
NR 54
TC 4
Z9 4
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2009
VL 702
IS 1
BP 340
EP 351
DI 10.1088/0004-637X/702/1/340
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BD
UT WOS:000269244500026
ER
PT J
AU Ross, NR
Assef, RJ
Kochanek, CS
Falco, E
Poindexter, SD
AF Ross, N. R.
Assef, R. J.
Kochanek, C. S.
Falco, E.
Poindexter, S. D.
TI THE UV-MID-IR SPECTRAL ENERGY DISTRIBUTION OF A z=1.7 QUASAR HOST GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; quasars: individual (SDSS J1004+4112)
ID SUPERMASSIVE BLACK-HOLES; GRAVITATIONALLY LENSED QUASAR; DIGITAL SKY
SURVEY; SDSS J1004+4112; TIME-DELAY; X-RAY; COSMOLOGICAL SIMULATIONS;
INFRARED LUMINOSITY; EDDINGTON RATIOS; ACTIVE GALAXIES
AB We have measured the spectral energy distribution (SED) of the host galaxy of the z(s) = 1.7 gravitationally lensed quasar SDSS J1004+4112 from 0.44-8.0 mu m (0.16-3.0 mu m in the rest frame). The large angular extent of the lensed images and their separation from the central galaxy of this cluster lens allows the images to be resolved even with the Spitzer Space Telescope. Based on the SED, the host galaxy is a mixture of relatively old and intermediate age stars with an inferred stellar mass of log(M-star/M-circle dot) = 11.09 +/- 0.28 and a star-formation rate of log((M) over dot/M-circle dot yr(-1)) = 1.21 +/- 0.26. Given the estimated black hole mass of M-BH similar or equal to 10(8.6) M-circle dot from locally calibrated correlations of black hole masses with line widths and luminosities, the black hole represents a fraction log(M-BH/M-star) = - 2.49 +/- 0.28 of the stellar mass and it is radiating at 0.24 +/- 0.05 of the Eddington limit. The ratio of the host stellar mass to the black hole mass is only marginally consistent with the locally observed ratio.
C1 [Ross, N. R.; Assef, R. J.; Kochanek, C. S.; Poindexter, S. D.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ross, NR (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
FU NASA [GO-9744, 10509, 10716, NAS5-2655, SST-20277]; NSF [AST-0708082]
FX We would like to thank C. Morgan and C. Peng for their comments and help
on the estimated black holemass. We would also like to thank D. Maoz and
M. Oguri for their comments. This work is based in part on observations
made with the NASA/ESA Hubble Space Telescope. Support for programs
GO-9744, 10509, and 10716 was provided by NASA through a grant from the
Space Telescope Science Institute, which is operated by AURA, Inc.,
under NASA contract NAS5-2655. It is also based in part on observations
made with the Spitzer Space Telescope, AO-20451, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. Support for this program SST-20277 was provided by
NASA through an award issued by JPL/Caltech. C. S. K. is also supported
by NSF grant AST-0708082.
NR 44
TC 8
Z9 8
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2009
VL 702
IS 1
BP 472
EP 479
DI 10.1088/0004-637X/702/1/472
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 487BD
UT WOS:000269244500038
ER
PT J
AU Qiu, KP
Zhang, QZ
AF Qiu, Keping
Zhang, Qizhou
TI DISCOVERY OF EXTREMELY HIGH VELOCITY "MOLECULAR BULLETS" IN THE HH 80-81
HIGH-MASS STAR-FORMING REGION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; ISM: individual (HH 80-81); ISM: jets and
outflows; masers; stars: early-type; stars: formation
ID SUBMILLIMETER ARRAY OBSERVATIONS; THERMAL RADIO JET; PROPER MOTIONS;
BIPOLAR OUTFLOWS; YOUNG STARS; HOT CORE; EMISSION; DISK; CONDENSATIONS;
ACCRETION
AB We present Submillimeter Array 1.3 mm waveband continuum and molecular line observations of the HH 80-81 high-mass star-forming region. The dust continuum emission reveals two dominant peaks, MM1 and MM2, and line emission from high-density tracers suggests the presence of another core, MC. Molecular line emission from MM1, which harbors the exciting source of the HH 80-81 radio jet, yields a hot molecular core at a gas temperature of 110 K. The two younger cores, MM2 and MC, both appear to power collimated CO outflows. In particular, the outflow arising from MM2 exhibits a jet-like morphology and a broad velocity range of 190 km s(-1). The outflow contains compact and fast moving molecular clumps, known as "molecular bullets," first discovered in low-mass class 0 protostellar outflows. These "bullets" cannot be locally entrained or swept up from the ambient gas, but are more likely ejected from the close vicinity of the central protostar. The discovery of this remarkable outflow manifests an episodic, disk-mediated accretion for massive star formation.
C1 [Qiu, Keping] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Qiu, Keping; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Qiu, KP (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
EM kqiu@cfa.harvard.edu; qzhang@cfa.harvard.edu
OI Zhang, Qizhou/0000-0003-2384-6589
NR 47
TC 21
Z9 21
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2009
VL 702
IS 1
BP L66
EP L71
DI 10.1088/0004-637X/702/1/L66
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 484NR
UT WOS:000269053200015
ER
PT J
AU Savcheva, A
Cirtain, JW
DeLuca, EE
Golub, L
AF Savcheva, A.
Cirtain, J. W.
DeLuca, E. E.
Golub, L.
TI DOES A POLAR CORONAL HOLE'S FLUX EMERGENCE FOLLOW A HALE-LIKE LAW?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: magnetic fields; Sun: X-rays, gamma rays
ID X-RAY TELESCOPE; HINODE MISSION; JETS; REGIONS; XRT
AB Recent increases in spatial and temporal resolution for solar telescopes sensitive to EUV and X-ray radiation have revealed the prevalence of transient jet events in polar coronal holes. Using data collected by the X-Ray Telescope on Hinode, Savcheva et al. confirmed the observation, made first by the Soft X-ray Telescope on Yohkoh, that some jets exhibit a motion transverse to the jet outflow direction. The velocity of this transverse motion is, on average, 10 km s(-1). The direction of the transverse motion, in combination with the standard reconnection model for jet production (e. g., Shibata et al.), reflects the magnetic polarity orientation of the ephemeral active region at the base of the jet. From this signature, we find that during the present minimum phase of the solar cycle the jet-base ephemeral active regions in the polar coronal holes had a preferred east-west direction, and that this direction reversed during the cycle's progression through minimum. In late 2006 and early 2007, the preferred direction was that of the active regions of the coming sunspot cycle (cycle 24), but in late 2008 and early 2009 the preferred direction has been that of the active regions of sunspot cycle 25. These findings are consistent with the observations of Wilson et al. suggesting that each cycle of solar activity begins at polar latitudes soon after the onset of the previous cycle.
C1 [Savcheva, A.; DeLuca, E. E.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cirtain, J. W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Savcheva, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 58, Cambridge, MA 02138 USA.
EM asavcheva@cfa.harvard.edu
RI DeLuca, Edward/L-7534-2013
OI DeLuca, Edward/0000-0001-7416-2895
FU NASA [NNM07AB07C]
FX Hinode is a Japanese mission developed, launched, and operated by
ISAS/JAXA in partnership with NAOJ, NASA, and STFC ( UK). Additional
operational support is provided by ESA, NSC (Norway). This work was
supported by NASA contract NNM07AB07C to SAO. We thank Dibyendu Nandi,
Piet Martens, Andres Munoz-Jeramillo, Ron Moore, and Julie Stern for
helpful discussions. We thank the referee for very useful comments and
suggestions that greatly helped to make this Letter better.
NR 18
TC 16
Z9 16
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 SEP 1
PY 2009
VL 702
IS 1
BP L32
EP L36
DI 10.1088/0004-637X/702/1/L32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 484NR
UT WOS:000269053200008
ER
PT J
AU Gutermuth, RA
Megeath, ST
Myers, PC
Allen, LE
Pipher, JL
Fazio, GG
AF Gutermuth, R. A.
Megeath, S. T.
Myers, P. C.
Allen, L. E.
Pipher, J. L.
Fazio, G. G.
TI A SPITZER SURVEY OF YOUNG STELLAR CLUSTERS WITHIN ONE KILOPARSEC OF THE
SUN: CLUSTER CORE EXTRACTION AND BASIC STRUCTURAL ANALYSIS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE infrared: stars; stars: formation; stars: pre-main sequence
ID STAR-FORMING REGIONS; INFRARED-ARRAY-CAMERA; HERBIG AE/BE STARS;
IN-FLIGHT PERFORMANCE; SPACE-TELESCOPE; MOLECULAR CLOUDS; INTERSTELLAR
CLOUDS; EMBEDDED CLUSTERS; IMAGING SURVEY; C2D SURVEY
AB We present a uniform mid-infrared imaging and photometric survey of 36 young, nearby, star-forming clusters and groups using Spitzer IRAC and MIPS. We have confidently identified and classified 2548 young stellar objects (YSOs) using recently established mid-infrared color-based methods. We have devised and applied a new algorithm for the isolation of local surface density enhancements from point source distributions, enabling us to extract the overdense cores of the observed star-forming regions for further analysis. We have compiled several basic structural measurements of these cluster cores from the data, such as mean surface densities of sources, cluster core radii, and aspect ratios, in order to characterize the ranges for these quantities. We find that a typical cluster core is 0.39 pc in radius, has 26 members with infrared excess in a ratio of Class II to Class I sources of 3.7, is embedded in a A(K) = 0.8 mag cloud clump, and has a surface density of 60 pc(-2). We examine the nearest neighbor distances among the YSOs in several ways, demonstrating similarity in the spacings between Class II and Class I sources but large member clusters appear more dense than smaller clusters. We demonstrate that near-uniform source spacings in cluster cores are common, suggesting that simple Jeans fragmentation of parsec-scale cloud clumps may be the dominant process governing star formation in nearby clusters and groups. Finally, we compare our results to other similar surveys in the literature and discuss potential biases in the data to guide further interpretation.
C1 [Gutermuth, R. A.; Myers, P. C.; Allen, L. E.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
RP Gutermuth, RA (reprint author), Smith Coll, Northampton, MA 01063 USA.
NR 92
TC 289
Z9 289
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2009
VL 184
IS 1
BP 18
EP 83
DI 10.1088/0067-0049/184/1/18
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AF
UT WOS:000269625100002
ER
PT J
AU Wright, NJ
Drake, JJ
AF Wright, N. J.
Drake, J. J.
TI THE MASSIVE STAR-FORMING REGION CYGNUS OB2. I. CHANDRA CATALOG OF
ASSOCIATION MEMBERS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE open clusters and associations: individual (Cygnus OB2); stars: pre-main
sequence; X-rays: stars
ID X-RAY FLARE; ORION ULTRADEEP PROJECT; GALACTIC PLANE IPHAS; H-ALPHA
SURVEY; YOUNG STARS; SPECTRAL CLASSIFICATION; PARAMETER-ESTIMATION;
CYG-OB2 ASSOCIATION; STELLAR POPULATION; EMISSION
AB We present a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations, was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. We used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric Ha survey, the Two Micron All Sky Survey, and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. Seven hundred and fifty seven (45%) of these objects have six-band r', H alpha, i', J, H, and K(s) optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source we estimate that our X-ray catalog includes <1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broadband fluxes, model fits, and optical and near-IR photometry in what is one of the largest X-ray catalog of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.
C1 [Wright, N. J.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nwright@head.cfa.harvard.edu
FU NASA [NAS8-39073]; SAO
FX J. J. D. was funded by NASA contract NAS8-39073 to the Chandra X-ray
Center (CXC) during the course of this research and thanks the CXC
director, Harvey Tananbaum, and the science team for advice and support.
N. J. W. acknowledges an SAO Pre-doctoral Fellowship.
NR 59
TC 18
Z9 18
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2009
VL 184
IS 1
BP 84
EP 99
DI 10.1088/0067-0049/184/1/84
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AF
UT WOS:000269625100003
ER
PT J
AU Elvis, M
Civano, F
Vignali, C
Puccetti, S
Fiore, F
Cappelluti, N
Aldcroft, TL
Fruscione, A
Zamorani, G
Comastri, A
Brusa, M
Gilli, R
Miyaji, T
Damiani, F
Koekemoer, AM
Finoguenov, A
Brunner, H
Urry, CM
Silverman, J
Mainieri, V
Hasinger, G
Griffiths, R
Carollo, M
Hao, H
Guzzo, L
Blain, A
Calzetti, D
Carilli, C
Capak, P
Ettori, S
Fabbiano, G
Impey, C
Lilly, S
Mobasher, B
Rich, M
Salvato, M
Sanders, DB
Schinnerer, E
Scoville, N
Shopbell, P
Taylor, JE
Taniguchi, Y
Volonteri, M
AF Elvis, Martin
Civano, Francesca
Vignali, Cristian
Puccetti, Simonetta
Fiore, Fabrizio
Cappelluti, Nico
Aldcroft, T. L.
Fruscione, Antonella
Zamorani, G.
Comastri, Andrea
Brusa, Marcella
Gilli, Roberto
Miyaji, Takamitsu
Damiani, Francesco
Koekemoer, Anton M.
Finoguenov, Alexis
Brunner, Hermann
Urry, C. M.
Silverman, John
Mainieri, Vincenzo
Hasinger, Guenther
Griffiths, Richard
Carollo, Marcella
Hao, Heng
Guzzo, Luigi
Blain, Andrew
Calzetti, Daniela
Carilli, C.
Capak, Peter
Ettori, Stefano
Fabbiano, Giuseppina
Impey, Chris
Lilly, Simon
Mobasher, Bahram
Rich, Michael
Salvato, Mara
Sanders, D. B.
Schinnerer, Eva
Scoville, N.
Shopbell, Patrick
Taylor, James E.
Taniguchi, Yoshiaki
Volonteri, Marta
TI THE CHANDRA COSMOS SURVEY. I. OVERVIEW AND POINT SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; cosmology: observations; galaxies: evolution; quasars:
general; surveys; X-rays: general
ID WIDE-FIELD SURVEY; BLACK-HOLE MASS; X-RAY SURVEY; EVOLUTION SURVEY
COSMOS; LYMAN BREAK GALAXIES; NORTH SURVEY; PHOTOMETRIC REDSHIFTS;
VELOCITY DISPERSION; NUMBER COUNTS; LOCKMAN-HOLE
AB The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.5 deg(2) of the COSMOS field (centered at 10(h), + 02 degrees) with an effective exposure of similar to 160 ks, and an outer 0.4 deg(2) area with an effective exposure of similar to 80 ks. The limiting source detection depths are 1.9 x 10(-16) erg cm(-2) s(-1) in the soft (0.5-2 keV) band, 7.3 x 10(-16) erg cm(-2) s(-1) in the hard (2-10 keV) band, and 5.7 x 10(-16) erg cm(-2) s(-1) in the full (0.5-10 keV) band. Here we describe the strategy, design, and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of <2 x 10(-5) (1655 in the full, 1340 in the soft, and 1017 in the hard bands). By using a grid of 36 heavily (similar to 50%) overlapping pointing positions with the ACIS-I imager, a remarkably uniform (+/- 12%) exposure across the inner 0.5 deg(2) field was obtained, leading to a sharply defined lower flux limit. The widely different point-spread functions obtained in each exposure at each point in the field required a novel source detection method, because of the overlapping tiling strategy, which is described in a companion paper. This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with subarcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper. The full catalog is described here in detail and is available online.
C1 [Elvis, Martin; Civano, Francesca; Aldcroft, T. L.; Fruscione, Antonella; Hao, Heng; Fabbiano, Giuseppina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vignali, Cristian] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Vignali, Cristian; Zamorani, G.; Comastri, Andrea; Gilli, Roberto; Ettori, Stefano] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Puccetti, Simonetta] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Puccetti, Simonetta; Fiore, Fabrizio] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Brusa, Marcella; Finoguenov, Alexis] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Miyaji, Takamitsu] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico.
[Miyaji, Takamitsu] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Damiani, Francesco] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy.
[Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Urry, C. M.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Silverman, John; Carollo, Marcella; Lilly, Simon] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Mainieri, Vincenzo] ESO, D-85748 Garching, Germany.
[Hasinger, Guenther] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Griffiths, Richard] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Guzzo, Luigi] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
[Blain, Andrew; Salvato, Mara; Scoville, N.; Shopbell, Patrick] CALTECH, Pasadena, CA 91125 USA.
[Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Carilli, C.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Impey, Chris] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Rich, Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Taylor, James E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Taniguchi, Yoshiaki] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Volonteri, Marta] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Cappelluti, Nico; Brusa, Marcella; Finoguenov, Alexis; Brunner, Hermann; Hasinger, Guenther] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Miyaji, T (reprint author), POB 439027, San Ysidro, CA 92143 USA.
RI Vignali, Cristian/J-4974-2012; Urry, Claudia/G-7381-2011; Ettori,
Stefano/N-5004-2015; Comastri, Andrea/O-9543-2015; Gilli,
Roberto/P-1110-2015;
OI Koekemoer, Anton/0000-0002-6610-2048; Schinnerer,
Eva/0000-0002-3933-7677; Brusa, Marcella/0000-0002-5059-6848; Damiani,
Francesco/0000-0002-7065-3061; Puccetti, Simonetta/0000-0002-2734-7835;
Fiore, Fabrizio/0000-0002-4031-4157; Vignali,
Cristian/0000-0002-8853-9611; Urry, Claudia/0000-0002-0745-9792; Ettori,
Stefano/0000-0003-4117-8617; Comastri, Andrea/0000-0003-3451-9970;
Gilli, Roberto/0000-0001-8121-6177; Cappelluti,
Nico/0000-0002-1697-186X; Zamorani, Giovanni/0000-0002-2318-301X
FU NASA Chandra [GO7-8136A]; NASA [NAS8-39073]; NASA/ADP [NNX07AT02G];
ASI/INAF [I/023/05/0, I/024/05/0, I/088/06]; PRIN/MUR [2006-02-5203];
Bundesministerium fur Bildung und Forschung/Deutsches Zentrum fur Luft
und Raumfahrt; Max Planck Society
FX This work was supported in part by NASA Chandra grant number GO7-8136A
(M. E., C. V., M. B., A. F.), NASA contract NAS8-39073 (Chandra X-ray
Center), and by NASA/ADP grant NNX07AT02G (TM at UCSD). In Italy this
work is supported by ASI/INAF contracts I/023/05/0, I/024/05/0 and
I/088/06, by PRIN/MUR grant 2006-02-5203. In Germany this project is
supported by the Bundesministerium fur Bildung und Forschung/Deutsches
Zentrum fur Luft und Raumfahrt and the Max Planck Society.
NR 65
TC 254
Z9 254
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2009
VL 184
IS 1
BP 158
EP 171
DI 10.1088/0067-0049/184/1/158
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 492AF
UT WOS:000269625100008
ER
PT J
AU Whiteford, N
Skelly, T
Curtis, C
Ritchie, ME
Lohr, A
Zaranek, AW
Abnizova, I
Brown, C
AF Whiteford, Nava
Skelly, Tom
Curtis, Christina
Ritchie, Matt E.
Loehr, Andrea
Zaranek, Alexander Wait
Abnizova, Irina
Brown, Clive
TI Swift: primary data analysis for the Illumina Solexa sequencing platform
SO BIOINFORMATICS
LA English
DT Article
ID MICROARRAYS
AB Motivation: Primary data analysis methods are of critical importance in second generation DNA sequencing. Improved methods have the potential to increase yield and reduce the error rates. Openly documented analysis tools enable the user to understand the primary data, this is important for the optimization and validity of their scientific work.
Results: In this article, we describe Swift, a new tool for performing primary data analysis on the Illumina Solexa Sequencing Platform. Swift is the first tool, outside of the vendors own software, which completes the full analysis process, from raw images through to base calls. As such it provides an alternative to, and independent validation of, the vendor supplied tool. Our results show that Swift is able to increase yield by 13.8%, at comparable error rate.
C1 [Whiteford, Nava; Skelly, Tom; Abnizova, Irina; Brown, Clive] Wellcome Trust Sanger Inst, Cambridge CB10 1SA, England.
[Curtis, Christina] Univ Cambridge, CRUK Cambridge Res Inst, Li Ka Shing Ctr, Dept Oncol, Cambridge CB2 0RE, England.
[Ritchie, Matt E.] Walter & Eliza Hall Inst Med Res, Bioinformat Div, Parkville, Vic 3052, Australia.
[Loehr, Andrea] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zaranek, Alexander Wait] Harvard Univ, Sch Med, Boston, MA 02115 USA.
RP Whiteford, N (reprint author), Oxford Nanopore Technol, Begbroke Sci Pk,Sandy Lane, Kidlington OX5 1PF, England.
EM new@sgenomics.org
OI Ritchie, Matthew/0000-0002-7383-0609
FU Wellcome Trust
NR 15
TC 43
Z9 44
U1 1
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1367-4803
J9 BIOINFORMATICS
JI Bioinformatics
PD SEP 1
PY 2009
VL 25
IS 17
BP 2194
EP 2199
DI 10.1093/bioinformatics/btp383
PG 6
WC Biochemical Research Methods; Biotechnology & Applied Microbiology;
Computer Science, Interdisciplinary Applications; Mathematical &
Computational Biology; Statistics & Probability
SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
Computer Science; Mathematical & Computational Biology; Mathematics
GA 486KX
UT WOS:000269196000008
PM 19549630
ER
PT J
AU Roubik, DW
Villanueva-Gutierrez, R
AF Roubik, David W.
Villanueva-Gutierrez, Rogel
TI Invasive Africanized honey bee impact on native solitary bees: a pollen
resource and trap nest analysis
SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE biodiversity; competition; mutualist networks; natural disturbance;
phylogenetic community organization; pollination; tropical biosphere
reserve
ID YUCATAN PENINSULA; TROPICAL FOREST; HYMENOPTERA; MEXICO; APIDAE;
POPULATIONS; COMPETITION; DIVERSITY; HURRICANE; SITE
AB Little is known of the potential coevolution of flowers and bees in changing, biodiverse environments. Female solitary bees, megachilids and Centris, and their nest pollen provisions were monitored with trap nests over a 17-year period in a tropical Mexican biosphere reserve. Invasion by feral Apis (i.e. Africanized honey bees) occurred after the study began, and major droughts and hurricanes occurred throughout. Honey bee competition, and ostensibly pollination of native plants, caused changes in local pollination ecology. Shifts in floral hosts by native bees were common and driven by plant phylogenetics, whereby plants of the same families or higher taxa were substituted for those dominated by honey bees or lost as a result of natural processes. Two important plant families, Anacardiaceae and Euphorbiaceae, were lost to competing honey bees, but compensated for by greater use of Fabaceae, Rubiaceae, and Sapotaceae among native bees. Natural disasters made a large negative impact on native bee populations, but the sustained presence of Africanized honey bees did not. Over 171 plant species comprised the pollen diets of the honey bees, including those most important to Centris and megachilids (72 and 28 species, respectively). Honey bee pollination of Pouteria (Sapotaceae) plausibly augmented the native bees' primary pollen resource and prevented their decline. Invasive generalist pollinators may, however, cause specialized competitors to fail, especially in less biodiverse environments. No claim to original US government works. Journal compilation (C) 2009 The Linnean Society of London, Biological Journal of the Linnean Society, 2009, 98, 152-160.
C1 [Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Panama.
[Villanueva-Gutierrez, Rogel] El Colegio Frontera ECOSUR, Quintana Roo, Mexico.
RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.
EM roubikd@si.edu
FU Smithsonian Institution Scholarly Studies
FX We thank W. Colli-Ucan and Margarito Tuz for field and laboratory
assistance; Dr. Terry Griswold for help with bee taxonomy; Smithsonian
Institution Scholarly Studies grants to DWR; Centro de Investigaciones
de Quintana Roo (CIQRO) and ECOSUR for general support; and J. H. Cane,
S. Sakai, Y. Basset, J. Wright, and anonymous reviewers for suggestions
on drafts of the manuscript.
NR 54
TC 30
Z9 30
U1 7
U2 68
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4066
EI 1095-8312
J9 BIOL J LINN SOC
JI Biol. J. Linnean Soc.
PD SEP
PY 2009
VL 98
IS 1
BP 152
EP 160
PG 9
WC Evolutionary Biology
SC Evolutionary Biology
GA 487YM
UT WOS:000269315600013
ER
PT J
AU Camacho, R
Boyero, L
Cornejo, A
Ibanez, A
Pearson, RG
AF Camacho, Regina
Boyero, Luz
Cornejo, Aydee
Ibanez, Alicia
Pearson, Richard G.
TI Local Variation in Shredder Distribution can Explain their Oversight in
Tropical Streams
SO BIOTROPICA
LA English
DT Article
DE altitude; Australian wet tropics; latitude; leaf litter breakdown;
macroinvertebrates; Panama
ID LEAF-LITTER BREAKDOWN; RAIN-FOREST STREAM; RIVER CONTINUUM CONCEPT;
ECOSYSTEM FUNCTION; FOOD-WEBS; BENTHIC MACROINVERTEBRATES;
FUNCTIONAL-ORGANIZATION; TROPHIC RELATIONSHIPS; WOODLAND STREAM; AQUATIC
INSECTS
AB Stream shredders play an important role in the breakdown of allochthonous leaf litter-a well-known, key process in temperate headwater streams. In contrast, it has been suggested that litter breakdown in tropical streams is driven by microorganisms, shredders being scarce or absent. We propose that shredders have been overlooked in some tropical streams for two reasons: (1) assuming that tropical shredders belong to the same taxa as temperate ones, without determining the diet of tropical litter fauna; and (2) the small spatial scale of most tropical stream studies, which do not account for intra- and inter-site comparisons. We explored shredder abundance and species richness in six streams in each of two tropical regions, the Australian wet tropics (AWT) and Panama (PAN), finding 734 individuals of 12 shredder species in AWT and 391 individuals of 16 species in PAN. Shredder species richness was positively related to altitude in AWT, but not in PAN. Shredder contribution to total leaf breakdown in the field was 24 +/- 3 SE percent in AWT and negligible in PAN, but this was probably due to the unsuccessful colonization of experimental cages by PAN shredders. In the laboratory, shredder contribution to total leaf breakdown was higher than in the field (35%+/- 2 SE in AWT and 64%+/- 3 SE in PAN) and varied with leaf decomposability. Our results support earlier indications that shredders are not scarce or functionally unimportant in the tropics, and suggest that their contribution to litter processing should be determined along altitudinal gradients.
C1 [Camacho, Regina; Boyero, Luz; Pearson, Richard G.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
[Boyero, Luz; Ibanez, Alicia] Smithsonian Trop Res Inst, Balboa 2072, Panama.
RP Boyero, L (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
EM luz.boyero@jcu.edu.au
RI Boyero, Luz/L-5822-2014;
OI Boyero, Luz/0000-0001-7366-9299; Pearson, Richard/0000-0001-6047-031X
FU Smithsonian Tropical Research Institute (STRI); Committee for Research
and Exploration of the National Geographic Society [7980-06]; James Cook
University; Comunidad de Madrid, Spain [GR/AMB/0744/2004]; ANAM; STRI
FX E. Bermingham provided facilities and support at the Smithsonian
Tropical Research Institute (STRI). R. AizprUa helped with leaf
collection. A. Almanza, C. McGrath and B. Ashley helped with shredder
collection. R. Holzenthal and Y. Aguila helped with shredder
identification. R. Urriola, J. Flores and other STRI staff provided
logistical support. The Autoridad Nacional del Ambiente (ANAM) provided
the necessary research and collecting permits in Panama. The study was
supported by grants from the Committee for Research and Exploration of
the National Geographic Society (Grant number 7980-06; P.I., LB) and
James Cook University. LB was supported by project GR/AMB/0744/2004 from
the Comunidad de Madrid, Spain (P.I., Pedro A. Rincon). AC and AI were
supported by contracts from ANAM and STRI (Panama), respectively.
NR 48
TC 18
Z9 19
U1 2
U2 14
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD SEP
PY 2009
VL 41
IS 5
BP 625
EP 632
DI 10.1111/j.1744-7429.2009.00519.x
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 492YZ
UT WOS:000269700500016
ER
PT J
AU Dattilo, W
Izzo, TJ
Inouye, BD
Vasconcelos, HL
Bruna, EM
AF Dattilo, Wesley
Izzo, Thiago J.
Inouye, Brian D.
Vasconcelos, Heraldo L.
Bruna, Emilio M.
TI Recognition of Host Plant Volatiles by Pheidole minutula Mayr
(Myrmicinae), an Amazonian Ant-Plant Specialist
SO BIOTROPICA
LA English
DT Article
DE ant-plant interactions; chemical cues; Formicidae; host-plant location;
Maieta guianensis; mutualisms; myrmecophytes
ID TRIBE MICONIEAE MELASTOMATACEAE; MACARANGA EUPHORBIACEAE; MUTUALISTIC
NETWORKS; SPECIES-SPECIFICITY; PROTECTION; QUEENS; COEVOLUTION;
INHABITANTS; FORMICIDAE; PHYLOGENY
AB In the tropics, several ant species are obligate inhabitants of leaf pouches and other specialized structures in plants known as myrmecophytes. However, the cues used by ant queens to locate suitable host-plants following dispersal remain poorly understood. Here we tested the hypothesis that Pheidole minutula queens use volatiles to distinguish their host Maieta guianensis (Melastomataceae) from other sympatric myrmecophytes. To do so, we used a Y-tube olfactometer to quantify the preference for volatiles of different plant species. Our results indicate that P. minutula queens discriminate the chemical volatiles produced by its host-plant from those of other sympatric ant-plant species. However, queens failed to distinguish the volatiles of Maieta from those of the ant-plant Tococa bullifera (Melastomataceae), with which P. minutula is not mutualistically associated. Nevertheless, a strong preference for Maieta over Tococa was observed during a subsequent bioassay, where the ants had physical contact with a domatium of each plant species. These results suggest that additional, short distance mechanisms are also necessary for host discrimination. Overall, our findings suggest that the high degree of compartmentalization observed in symbiotic ant-plant relationships is achieved, at least in part, by the relatively high degree of specificity in host selection displayed by foundress queens.
C1 [Dattilo, Wesley; Izzo, Thiago J.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil.
[Dattilo, Wesley; Izzo, Thiago J.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil.
[Izzo, Thiago J.; Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA.
[Inouye, Brian D.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA.
[Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38400 Uberlandia, MG, Brazil.
[Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA.
[Dattilo, Wesley] Univ Estadual Norte Fluminense, Ctr Biociencias & Biotecnol, Campos, RJ, Brazil.
RP Izzo, TJ (reprint author), Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil.
EM izzothiago@gmail.com
RI Dattilo, Wesley/A-6371-2012; Bruna, Emilio/H-2769-2012; Vasconcelos,
Heraldo/C-3353-2013; Izzo, Thiago/K-7405-2012
OI Dattilo, Wesley/0000-0002-4758-4379; Bruna, Emilio/0000-0003-3381-8477;
Vasconcelos, Heraldo/0000-0001-6969-7131; Izzo,
Thiago/0000-0002-4613-3787
FU Brazil's Conselho Nacional de Desenvolvimento Cientifico e Tecnologic
[552680/2006-0, 490518/2006-0]; US National Science Foundation
[DEB-0452720, DEB-0453631]
FX We thank D. Yu and P. R. Guimaraes, and two anonymous reviewers for
comments on the manuscript and the Chemical Department of UFAM for
assistance with the experiments. Financial support was provided by
Brazil's Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
(Grants 552680/2006-0 and 490518/2006-0 to TJI), and the US National
Science Foundation (grants DEB-0452720 and DEB-0453631 to EMB and BDI).
This is publication 525 in the BDFFP technical series.
NR 35
TC 9
Z9 10
U1 1
U2 18
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD SEP
PY 2009
VL 41
IS 5
BP 642
EP 646
DI 10.1111/j.1744-7429.2009.00518.x
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 492YZ
UT WOS:000269700500018
ER
PT J
AU Metcalf, CJE
McMahon, SM
Clark, JS
AF Metcalf, C. Jessica E.
McMahon, Sean M.
Clark, James S.
TI Overcoming data sparseness and parametric constraints in modeling of
tree mortality: a new nonparametric Bayesian model
SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE
FORESTIERE
LA English
DT Article
ID SAPLING MORTALITY; BRITISH-COLUMBIA; TROPICAL FORESTS; DIAMETER GROWTH;
SHADE TOLERANCE; PLOT DATA; RATES; DYNAMICS; HISTORY; SPRUCE
AB Accurately describing patterns of tree mortality is central to understanding forest dynamics and is important for both management and ecological inference. However, for many tree species, annual survival of most individuals is high, so that mortality is rare and, therefore, difficult to estimate. Furthermore, tree mortality models have potentially complex suites of covariates. Here, we extend traditional and recent approaches to modeling tree mortality and propose a new nonparametric Bayesian method. Our model is constrained to both reflect and distinguish known relationships between mortality and its two key covariates, diameter and diameter increment growth, but it remains sufficiently flexible to capture a wide variety of patterns of mortality across these covariates. Our model also allows incorporation of outside information in the form of priors, so that increased mortality of large trees can always be formally modeled even when data are sparse. We present results for our nonparametric Bayesian mortality model for maple (Acer spp.), holly (Ilex spp.), sweet gum (Liquidambar styraciflua L.), and tulip-poplar (Liriodendron tulipifera L.) populations from North Carolina, USA.
C1 [Metcalf, C. Jessica E.] Penn State Univ, Ctr Infect Dis Dynam, State Coll, PA 16801 USA.
[McMahon, Sean M.; Clark, James S.] Smithsonian Environm Res Ctr, Smithsonian Trop Res Inst, Edgewater, MD 21307 USA.
[Clark, James S.] Duke Univ, Dept Biol, Durham, NC 27707 USA.
[Clark, James S.] Duke Univ, Dept Stat Sci, Durham, NC 27707 USA.
RP Metcalf, CJE (reprint author), Princeton Univ, Dept Ecol & Evolut Biol, Eno Hall, Princeton, NJ 08544 USA.
EM cjm29@duke.edu
RI Clark, James/G-6331-2011
NR 48
TC 20
Z9 21
U1 2
U2 18
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0045-5067
J9 CAN J FOREST RES
JI Can. J. For. Res.-Rev. Can. Rech. For.
PD SEP
PY 2009
VL 39
IS 9
BP 1677
EP 1687
DI 10.1139/X09-083
PG 11
WC Forestry
SC Forestry
GA 494RY
UT WOS:000269834400005
ER
PT J
AU Duda, TF
Lessios, HA
AF Duda, T. F., Jr.
Lessios, H. A.
TI Connectivity of populations within and between major biogeographic
regions of the tropical Pacific in Conus ebraeus, a widespread marine
gastropod
SO CORAL REEFS
LA English
DT Article
DE Phylogeography; East Pacific Barrier; Conus; Gene flow; Population
structure
ID INDO-WEST PACIFIC; HIGH-DISPERSAL STARFISH; CORAL-REEF FISH;
GENETIC-STRUCTURE; MITOCHONDRIAL-DNA; OCEAN CURRENTS; EVOLUTIONARY
HISTORY; FAUNAL AFFINITIES; CHANOS-CHANOS; EASTERN
AB Information on genetic connectivity and structure of populations in the tropical Pacific is critical for making inferences about the origins and maintenance of diversity in this region. Sequences of the mitochondrial COI gene from 92 individuals of the trans-Pacific gastropod Conus ebraeus from eight localities spanning the tropical Pacific were analyzed to determine whether populations in the western, central, and eastern Pacific exhibit genetic structure, to examine the demographic histories of populations, and to infer patterns of gene flow. A total of 43 unique haplotypes were recovered, including a common haplotype that occurred in six of the eight populations examined. AMOVA and pairwise F-statistics showed that populations in the western and central Pacific were significantly differentiated from populations in the eastern Pacific, but no other evidence of structure. Bayesian isolation-migration (IM) analysis suggested that populations in the western and central Pacific separated from those in eastern Pacific during the Pleistocene. Examination of mismatch distributions and results from IM revealed that populations in the western and central Pacific expanded during the Pleistocene. Gene flow across the East Pacific Barrier appears to occur predominantly westward.
C1 [Duda, T. F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Duda, T. F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
[Duda, T. F., Jr.; Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Duda, TF (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 1109 Geddes Ave, Ann Arbor, MI 48109 USA.
EM tfduda@umich.edu
FU NSF [0718370]; University of Michigan Museum of Zoology; Department of
Ecology and Evolutionary Biology
FX Dan Lindstrom, Laura Geyer, Alan Kohn, Steve Vollmer, Kirstie Kaiser,
and Hank Chaney assisted in obtaining or aided in access to specimens.
Don Barclay and family greatly assisted in fieldwork and collections in
American Samoa. Mike Hadfield and members of the Kewalo Marine Lab
(University of Hawaii) facilitated collections on Oahu. The crew of the
R/V Urraca (STRI) assisted with obtaining specimens from Panama. We are
extremely grateful for access to specimens from the Invertebrate Zoology
collections at the Santa Barbara Museum of Natural History. We also
appreciate comments on this manuscript from Diarmaid O Foighil, Evan
Braswell and several anonymous reviewers. Aspects of this work were
initiated while TFD was a Tupper Fellow at STRI and completed with
support from NSF (0718370) and start-up funds from the University of
Michigan Museum of Zoology and Department of Ecology and Evolutionary
Biology.
NR 70
TC 19
Z9 19
U1 0
U2 13
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
J9 CORAL REEFS
JI Coral Reefs
PD SEP
PY 2009
VL 28
IS 3
BP 651
EP 659
DI 10.1007/s00338-009-0485-9
PG 9
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 474ZN
UT WOS:000268323800010
ER
PT J
AU Thamm, S
Kalko, EKV
Wells, K
AF Thamm, Sven
Kalko, Elisabeth K. V.
Wells, Konstans
TI Ectoparasite Infestations of Hedgehogs (Erinaceus europaeus) are
Associated with Small-Scale Landscape Structures in an Urban-Suburban
Environment
SO ECOHEALTH
LA English
DT Article
DE Landscape structure; Ixodes; Host-parasite interaction; Macroparasite
epidemics; Matrix heterogeneity; Spatial epidemiology; Urbanization
ID LYME-DISEASE RISK; PARASITE TRANSMISSION; HABITAT FRAGMENTATION; FOREST
FRAGMENTATION; HOST POPULATIONS; GREAT-BRITAIN; PATTERNS; HETEROGENEITY;
ECOLOGY; DETERMINANTS
AB Animals that exploit heterogeneous and patchy environments encounter different local habitat conditions that influence their interaction with the environment, such as the acquisition of parasites. How and at which scales interaction processes between parasites, hosts, and the environment are realized remains largely unknown. We examined the infestation patterns of 56 hedgehogs (Erinaceus europaeus) with fleas and ticks at a small spatial scale within a 12 km(2) area along a suburban-urban gradient in southwestern Germany. The structure and type of habitats surrounding hedgehog capture locations were estimated from digital land cover data within radii of 20, 50, and 100 m. These were assumed to match the ranging area and underlying heterogeneous landscape matrix in which host-parasite interactions take place. Landscape-based models suggested that flea burdens significantly decreased with the diversity and heterogeneity of land cover, as well as with the areal coverage of roads within radii of 50 and 100 m. Overall tick infestation levels were mostly explained by the number of arable patches and the areal coverage of roads within radii of 50 and 100 m, as well as date of capture. Examination of the semivariance in model residuals revealed no evident spatial structure in any of the models with flea or tick infestation patterns as response variables. Our results, which are based on a sampling scheme within a relatively small spatio-temporal window, suggest that heterogeneous landscape matrices affect parasitization rates of animals in urban environments, with clear differences at the individual level.
C1 [Thamm, Sven; Kalko, Elisabeth K. V.; Wells, Konstans] Univ Ulm, Inst Expt Ecol, D-89081 Ulm, Germany.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Wells, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89081 Ulm, Germany.
EM konstans.wells@uni-ulm.de
RI Wells, Konstans/A-7232-2010
OI Wells, Konstans/0000-0003-0377-2463
NR 40
TC 9
Z9 11
U1 1
U2 18
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1612-9202
J9 ECOHEALTH
JI EcoHealth
PD SEP
PY 2009
VL 6
IS 3
BP 404
EP 413
DI 10.1007/s10393-009-0268-3
PG 10
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 605LC
UT WOS:000278348100012
PM 20119687
ER
PT J
AU Rompre, G
Robinson, WD
Desrochers, A
Angehr, G
AF Rompre, Ghislain
Robinson, W. Douglas
Desrochers, Andre
Angehr, George
TI Predicting declines in avian species richness under nonrandom patterns
of habitat loss in a Neotropical landscape
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE bird species richness; fragmentation; habitat degradation; habitat loss
scenarios; Neotropical rain forests; nonrandom patterns; Panama Canal
corridor; species-area relationship; species loss threshold; tropical
biodiversity
ID BARRO-COLORADO ISLAND; FOREST BIRD COMMUNITY; AREA RELATIONSHIP;
EXTINCTION DEBT; LAND-USE; PANAMA; BIODIVERSITY; FRAGMENTATION;
DEFORESTATION; FUTURE
AB One of the key concerns in conservation is to document and predict the effects of habitat loss on species richness. To do this, the species-area relationship (SAR) is frequently used. That relationship assumes random patterns of habitat loss and species distributions. In nature, however, species distribution patterns are usually nonrandom, influenced by biotic and abiotic factors. Likewise, socioeconomic and environmental factors influence habitat loss and are not randomly distributed across landscapes. We used a recently developed SAR model that accounts for nonrandomness to predict rates of bird species loss in fragmented forests of the Panama Canal region, an area that was historically covered in forest but now has 53% forest cover. Predicted species loss was higher than that predicted by the standard SAR. Furthermore, a species loss threshold was evident when remaining forest cover declined by 25%. This level of forest cover corresponds to 40% of the historical forest cover, and our model predicts rapid species loss past that threshold. This study illustrates the importance of considering patterns of species distributions and realistic habitat loss scenarios to develop better estimates of losses in species richness. Forecasts of tropical biodiversity loss generated from simple species-area relationships may underestimate actual losses because nonrandom patterns of species distributions and habitat loss are probably not unique to the Panama Canal region.
C1 [Rompre, Ghislain; Desrochers, Andre] Univ Laval, Ctr Etud Foret, Quebec City, PQ G1V 0A6, Canada.
[Rompre, Ghislain; Robinson, W. Douglas] Oregon State Univ, Dept Fisheries & Wildlife, Oak Creek Lab Biol, Corvallis, OR 97331 USA.
[Angehr, George] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
RP Rompre, G (reprint author), Univ Laval, Ctr Etud Foret, Pavillon Abitibi Price,2405 Rue Terrasse, Quebec City, PQ G1V 0A6, Canada.
EM ghislain.rompre.1@ulaval.ca
RI Desrochers, Andre/B-6248-2008
OI Desrochers, Andre/0000-0002-5676-964X
FU Natural Sciences and Engineering Research Council of Canada
FX This study was supported by the Natural Sciences and Engineering
Research Council of Canada, via a Ph.D. fellowship to G. Rompre.
Research in Panama was possible thanks to the generous help of the
Smithsonian Tropical Research Institute (STRI), Autoridad Nacional del
Ambiante (ANAM), Autoridad del Canal de Panama (ACP), Autoridad de la
Region Interoceanica (ARI), Centro de Estudio de Accion Social Panameno
(CEASPA), Fundo Peregrino Panama (FPP), and Contraloria General de la
Republica de Panama. We also thank Elena de Lombardo, Maria Leone, Oris
Ovecedo, Benjamen Ordonez (STRI), Charlotte Elton (CEASPA), Sayda de
Grimaldo (ARI), Anjel Muela (FPP), Pascual Fiengo, Jose and Gladys
Isturain, and Jeovanna Lowe for making things easier in the field by
giving access and helping to coordinate and organize the fieldwork. Eric
Seabloom, Marc-Andre Villard, Mathieu Bouchard, and Louis Belanger
brought helpful comments to the discussion and statistical analysis.
NR 95
TC 5
Z9 5
U1 1
U2 32
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD SEP
PY 2009
VL 19
IS 6
BP 1614
EP 1627
DI 10.1890/08-1207.1
PG 14
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 484VC
UT WOS:000269075200021
PM 19769107
ER
PT J
AU Gotelli, NJ
Anderson, MJ
Arita, HT
Chao, A
Colwell, RK
Connolly, SR
Currie, DJ
Dunn, RR
Graves, GR
Green, JL
Grytnes, JA
Jiang, YH
Jetz, W
Lyons, SK
McCain, CM
Magurran, AE
Rahbek, C
Rangel, TFLVB
Soberon, J
Webb, CO
Willig, MR
AF Gotelli, Nicholas J.
Anderson, Marti J.
Arita, Hector T.
Chao, Anne
Colwell, Robert K.
Connolly, Sean R.
Currie, David J.
Dunn, Robert R.
Graves, Gary R.
Green, Jessica L.
Grytnes, John-Arvid
Jiang, Yi-Huei
Jetz, Walter
Lyons, S. Kathleen
McCain, Christy M.
Magurran, Anne E.
Rahbek, Carsten
Rangel, Thiago F. L. V. B.
Soberon, Jorge
Webb, Campbell O.
Willig, Michael R.
TI Patterns and causes of species richness: a general simulation model for
macroecology
SO ECOLOGY LETTERS
LA English
DT Review
DE Biogeography; geographical range; macroecology; mechanistic simulation
modelling; mid-domain effect; species richness
ID WATER-ENERGY DYNAMICS; LATITUDINAL DIVERSITY GRADIENT; CLIMATE-CHANGE;
HISTORICAL BIOGEOGRAPHY; GEOMETRIC CONSTRAINTS; SPATIAL-PATTERNS;
BIOLOGICAL RELATIVITY; CONSERVATION BIOLOGY; PHYLOGENETIC SIGNAL; GLOBAL
BIODIVERSITY
AB Understanding the causes of spatial variation in species richness is a major research focus of biogeography and macroecology. Gridded environmental data and species richness maps have been used in increasingly sophisticated curve-fitting analyses, but these methods have not brought us much closer to a mechanistic understanding of the patterns. During the past two decades, macroecologists have successfully addressed technical problems posed by spatial autocorrelation, intercorrelation of predictor variables and non-linearity. However, curve-fitting approaches are problematic because most theoretical models in macroecology do not make quantitative predictions, and they do not incorporate interactions among multiple forces. As an alternative, we propose a mechanistic modelling approach. We describe computer simulation models of the stochastic origin, spread, and extinction of species' geographical ranges in an environmentally heterogeneous, gridded domain and describe progress to date regarding their implementation. The output from such a general simulation model (GSM) would, at a minimum, consist of the simulated distribution of species ranges on a map, yielding the predicted number of species in each grid cell of the domain. In contrast to curve-fitting analysis, simulation modelling explicitly incorporates the processes believed to be affecting the geographical ranges of species and generates a number of quantitative predictions that can be compared to empirical patterns. We describe three of the 'control knobs' for a GSM that specify simple rules for dispersal, evolutionary origins and environmental gradients. Binary combinations of different knob settings correspond to eight distinct simulation models, five of which are already represented in the literature of macroecology. The output from such a GSM will include the predicted species richness per grid cell, the range size frequency distribution, the simulated phylogeny and simulated geographical ranges of the component species, all of which can be compared to empirical patterns. Challenges to the development of the GSM include the measurement of goodness of fit (GOF) between observed data and model predictions, as well as the estimation, optimization and interpretation of the model parameters. The simulation approach offers new insights into the origin and maintenance of species richness patterns, and may provide a common framework for investigating the effects of contemporary climate, evolutionary history and geometric constraints on global biodiversity gradients. With further development, the GSM has the potential to provide a conceptual bridge between macroecology and historical biogeography.
C1 [Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA.
[Anderson, Marti J.] Massey Univ, Inst Informat & Math Stat, Auckland, New Zealand.
[Arita, Hector T.] Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City 04510, DF, Mexico.
[Arita, Hector T.] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Mexico City 04510, DF, Mexico.
[Chao, Anne] Natl Tsing Hua Univ, Inst Stat, Hsinchu 30043, Taiwan.
[Colwell, Robert K.; Rangel, Thiago F. L. V. B.; Willig, Michael R.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.
[Connolly, Sean R.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia.
[Connolly, Sean R.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
[Currie, David J.] Univ Ottawa, Dept Biol, Ottawa, ON K1N 6N5, Canada.
[Dunn, Robert R.] N Carolina State Univ, Dept Biol, Raleigh, NC 27607 USA.
[Dunn, Robert R.] N Carolina State Univ, Keck Ctr Behav Biol, Raleigh, NC 27607 USA.
[Graves, Gary R.] Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20013 USA.
[Green, Jessica L.] Univ Oregon, Dept Biol, Eugene, OR 97403 USA.
[Grytnes, John-Arvid] Univ Bergen, Dept Biol, N-5007 Bergen, Norway.
[Jiang, Yi-Huei] Natl Tsing Hua Univ, Inst Stat, Hsinchu 30043, Taiwan.
[Jetz, Walter] Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA.
[McCain, Christy M.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[McCain, Christy M.] Univ Colorado, CU Nat Hist Museum, Boulder, CO 80309 USA.
[Magurran, Anne E.] Univ St Andrews, Sch Biol, Gatty Marine Lab, St Andrews KY16 8LB, Fife, Scotland.
[Rahbek, Carsten] Univ Copenhagen, Inst Biol, Ctr Macroecol, DK-2100 Copenhagen 0, Denmark.
[Soberon, Jorge] Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66045 USA.
[Webb, Campbell O.] Harvard Univ Hebaria, Cambridge, MA 02138 USA.
[Willig, Michael R.] Univ Connecticut, Ctr Environm Sci & Engn, Storrs, CT 06269 USA.
RP Gotelli, NJ (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA.
EM ngotelli@uvm.edu
RI Colwell, Robert/C-7276-2015; Soberon, Jorge/N-7444-2015; Connolly,
Sean/E-7773-2011; Green, Jessica/C-4828-2009; Rangel,
Thiago/H-8708-2012; ARITA, HECTOR/I-6161-2012; Dunn, Robert/B-1360-2013;
Magurran, Anne/D-7463-2013; Rahbek, Carsten/D-9372-2013; Rahbek,
Carsten/L-1129-2013; Grytnes, John-Arvid/L-6357-2013
OI Soberon, Jorge/0000-0003-2160-4148; Connolly, Sean/0000-0003-1537-0859;
Currie, David J./0000-0002-4906-2363; Webb,
Campbell/0000-0003-1031-3249;
FU National Center for Ecological Analysis and Synthesis; NSF [DEB-0553768,
DEB-0541936, DEB-0072702]; University of California, Santa Barbara and
the State of California; Australian Research Council Environmental
Futures Network
FX This study is a contribution of the Synthetic Macroecological Models of
Species Diversity Working Group supported by the National Center for
Ecological Analysis and Synthesis, a Center funded by NSF (Grant
#DEB-0553768), the University of California, Santa Barbara and the State
of California. Additional funding for group meetings was provided by the
Australian Research Council Environmental Futures Network. Gotelli was
supported by NSF DEB-0541936, and Colwell and Rangel were supported by
NSF DEB-0072702. We thank D. Nogues-Bravo, W. Thuiller and two anonymous
referees for comments that improved the manuscript.
NR 113
TC 109
Z9 112
U1 7
U2 187
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD SEP
PY 2009
VL 12
IS 9
BP 873
EP 886
DI 10.1111/j.1461-0248.2009.01353.x
PG 14
WC Ecology
SC Environmental Sciences & Ecology
GA 483LU
UT WOS:000268969100002
PM 19702748
ER
PT J
AU Kula, RR
Lill, JT
Murphy, SM
Stoepler, T
AF Kula, Robert R.
Lill, John T.
Murphy, Shannon M.
Stoepler, Teresa
TI FIRST HOST RECORDS FOR THE NEARCTIC SPECIES TRIRAPHIS DISCOIDEUS
(HYMENOPTERA: BRACONIDAE: ROGADINAE)
SO ENTOMOLOGICAL NEWS
LA English
DT Article
DE American beech; black cherry; black gum; Limacodidae; Nearctic; northern
red oak; parasitoid; phenology; pignut hickory; Triraphis harrisinae;
white oak
ID PHYLOGENY
AB Limacodid larvae were collected from 2004 2007 on leaves of the following host plants in the District of Columbia and Maryland: Carya glabra, pignut hickory; Quercus alba, white oak; Quercus rubra, northern red oak; Nyssa sylvatica, black gum; Prunus serotina, black cherry; and Fagus grandifolia, American beech. Field-collected larvae were brought to the laboratory where they were kept in isolation for the purpose of rearing parasitoids. The rogadine braconid Triraphis discoideus (Cresson) was reared from the following host-host plant combinations: Acharia stimulea (Clemens), Adoneta spinuloides (Herrich-Schaffer), Lithacodes fasciola (Herrich-Schaffer), and Parasa chloris (Moore) on red oak; Euclea delphinii (Boisduval) on black gum and red oak; Isa textula (Herrich-Schaffer) on American beech, red oak, and white oak; Natada nasoni (Grote) on American beech, black gum, red oak, and white oak; Prolimacodes badia Hubner on black cherry and red oak; and an undetermined species of Tortricidia Packard on American beech. Host use was previously unknown for T. discoideus. Host use and phenology are discussed for Triraphis harrisinae (Ashmead), the only other described species of Triraphis in the Nearctic Region.
C1 [Kula, Robert R.] Agr Res Serv, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Lill, John T.; Murphy, Shannon M.; Stoepler, Teresa] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.
RP Kula, RR (reprint author), Agr Res Serv, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM Robert.Kula@ars.usda.gov; lillj@gwu.edu; smurph@gwu.edu;
stoepler@gwu.edu
FU National Science Foundation [DEB-0823274]; George Washington University;
Washington Biologists' Field Club
FX We thank Michael G. Pogue (Systematic Entomology Laboratory [SEL]), F.
Christian Thompson (SEL), and Scott R. Shaw (University of
Wyoming-Laramie) for reviewing the manuscript. We are especially
grateful to Scott Shaw for providing information on host use. Marie Metz
(SEL) captured the image. Funding for field collection and larval
rearing came from grants to JTL from the following organizations:
National Science Foundation DEB-0823274, The George Washington
University Facilitating Fund, and the Washington Biologists' Field Club.
NR 17
TC 4
Z9 4
U1 0
U2 1
PU AMER ENTOMOL SOC
PI PHILADELPHIA
PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA
SN 0013-872X
J9 ENTOMOL NEWS
JI Entomol. News
PD SEP-OCT
PY 2009
VL 120
IS 4
BP 380
EP 386
DI 10.3157/021.120.0406
PG 7
WC Entomology
SC Entomology
GA 596OW
UT WOS:000277695600007
ER
PT J
AU Whigham, DF
Verhoeven, JTA
Samarkin, V
Megonigal, PJ
AF Whigham, Dennis F.
Verhoeven, Jos T. A.
Samarkin, Vladimir
Megonigal, Patrick J.
TI Responses of Avicennia germinans (Black Mangrove) and the Soil Microbial
Community to Nitrogen Addition in a Hypersaline Wetland
SO ESTUARIES AND COASTS
LA English
DT Article
DE Avicennia germinans; Mangrove; Florida; Denitrification; Nitrogen
fixation; Microbial community
ID INDIAN RIVER LAGOON; VS. PHOSPHORUS LIMITATION; NUTRIENT ENRICHMENT;
RHIZOPHORA-MANGLE; HYDRAULIC CONDUCTIVITY; ACETYLENE-REDUCTION;
INORGANIC NITROGEN; FOREST STRUCTURE; TERMINOS LAGOON; OXIDE FLUXES
AB The responses of dwarf black mangroves (Avicennia germinans) and components of the microbial community to the addition of nitrate over a 2-year period were examined. The field study was conducted in the Indian River Lagoon (Florida) in a mangrove-dominated impoundment that was established for purposes of mosquito control. The responses of mangroves to the regular addition of nitrate were insignificant or relatively minor compared to responses of the components of the microbial community. Denitrification rates, measured in the field and laboratory, increased significantly in fertilized plots and nitrous oxide emission rates were almost six times higher in fertilized plots. Nitrogen fixation was significantly lower in fertilized plots. Results suggest that mangrove systems in the N-limited Indian River Lagoon are likely to be long-term sinks for any increases in N loading.
C1 [Whigham, Dennis F.; Samarkin, Vladimir; Megonigal, Patrick J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Verhoeven, Jos T. A.] Univ Utrecht, Inst Environm Biol, NL-3508 TB Utrecht, Netherlands.
RP Whigham, DF (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM whighamd@si.edu
RI Verhoeven, Jos/B-9514-2011;
OI Whigham, Dennis/0000-0003-1488-820X
FU Smithsonian Marine Station at Ft. Pierce (SMSFP)
FX The research was supported by grants from the Smithsonian Marine Station
at Ft. Pierce (SMSFP) and by resources of the Smithsonian Environmental
Research Center and Utrecht University. We thank Paul van der Ven, Kim
Givler, Amy Wolf, and Jay O'Neill for assistance with the field work and
analytical processing of samples. Special thanks to Val Paul, Woody Lee,
and support staff at SMSFP for ensuring the success of the project.
NR 50
TC 7
Z9 10
U1 1
U2 25
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
EI 1559-2731
J9 ESTUAR COAST
JI Estuaries Coasts
PD SEP
PY 2009
VL 32
IS 5
BP 926
EP 936
DI 10.1007/s12237-009-9184-6
PG 11
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 482PP
UT WOS:000268901500008
ER
PT J
AU Poulsen, M
Fernandez-Marin, H
Currie, CR
Boomsma, JJ
AF Poulsen, Michael
Fernandez-Marin, Hermogenes
Currie, Cameron R.
Boomsma, Jacobus J.
TI EPHEMERAL WINDOWS OF OPPORTUNITY FOR HORIZONTAL TRANSMISSION OF FUNGAL
SYMBIONTS IN LEAF-CUTTING ANTS
SO EVOLUTION
LA English
DT Article
DE Acromyrmex; basidiomycota; fungus-growing ants; host-symbiont
specificity; incompatibility; symbiont transmission
ID ATTA-CEPHALOTES L; GROWING ANTS; BACTERIAL SYMBIONTS; NEST
ESTABLISHMENT; ACROMYRMEX; EVOLUTION; FORMICIDAE; ATTINI; HYMENOPTERA;
COOPERATION
AB Evolutionary theory predicts that hosts are selected to prevent mixing of genetically different symbionts when competition among lineages reduces the productivity of a mutualism. The symbionts themselves may also defend their interests: recent studies of Acromyrmex leaf-cutting ants showed that somatic incompatibility enforces single-clone gardens within mature colonies, thereby constraining horizontal transmission of fungal symbionts. However, phylogenetic analyses indicate that symbiont switches occur frequently enough to remove most signs of host-symbiont cocladogenesis. Here we resolve this paradox by showing that transmission among newly founded Acromyrmex colonies is not constrained. All tested queens of sympatric A. octospinosus and A. echinatior offered a novel fragment of fungus garden accepted the new symbiont. The outcome was unaffected by genetic distance between the novel and the original symbiont, and by the ant species the novel symbiont came from. The colony founding stage may thus provide an efficient but transient window for horizontal transmission, in which the fungus is unable to actively defend its partnership position before the host feeds on it, so that host fecal droplets remain compatible with alternative strains during the early stage of colony founding. We discuss how brief stages of low commitment between partners may increase the evolutionary stability of ancient coevolved mutualisms.
C1 [Poulsen, Michael; Fernandez-Marin, Hermogenes; Boomsma, Jacobus J.] Univ Copenhagen, Ctr Social Evolut, Dept Biol, DK-2100 Copenhagen, Denmark.
[Poulsen, Michael; Fernandez-Marin, Hermogenes] Smithsonian Trop Res Inst, APO, AA 34002 USA.
[Poulsen, Michael; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA.
RP Poulsen, M (reprint author), Univ Copenhagen, Ctr Social Evolut, Dept Biol, Univ Pk 15, DK-2100 Copenhagen, Denmark.
EM Poulsen@bact.wisc.edu; FernandezH@si.edu; Currie@bact.wisc.edu;
JJBoomsma@bio.ku.dk
RI Boomsma, Jacobus/M-2785-2014; Poulsen, Michael/C-6276-2012
OI Boomsma, Jacobus/0000-0002-3598-1609; Poulsen,
Michael/0000-0002-2839-1715
FU Lundbeck Foundation; NSF [DEB-0747002]; Danish National Research
Foundation
FX We thank S. A. O. Armitage, A. Little, A. M. Schmidt, J. M. Thomas, and
L. V. Ugelvig for assistance with the collection of queens and setting
up the experiments, S. A. O. Armitage for the picture shown in Figure
1B, S. Adams and H. A. Horn for assistance with DNA extraction and PCR
amplification, G. Nachman and J. S. Pedersen for statistical advice, D.
K. Aanen, E. Caldera, N. Gerardo, J. Scott, J. M. Thomas, Associate
Editor C. Nice, and two anonymous reviewers for comments on a previous
draft of the manuscript, the Smithsonian Tropical Research Institute
(STRI) for providing logistic help and facilities to work in Gamboa and
for shortterm fellowships awarded to MP and HFM, and the Autoridad
Nacional del Ambiente y el Mar (ANAM) for permission to sample ant
colonies in Panama. Our study was supported by the Lundbeck Foundation
(MP), NSF grant DEB-0747002 (CC), and the Danish National Research
Foundation (JJB).
NR 68
TC 14
Z9 14
U1 0
U2 9
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD SEP
PY 2009
VL 63
IS 9
BP 2235
EP 2247
DI 10.1111/j.1558-5646.2009.00704.x
PG 13
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 488RJ
UT WOS:000269367200004
PM 19473381
ER
PT J
AU Petaev, MI
Jacobsen, SB
AF Petaev, Michail I.
Jacobsen, Stein B.
TI Petrologic study of SJ101, a new forsterite-bearing CAI from the Allende
CV3 chondrite
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ALUMINUM-RICH INCLUSIONS; CARBONACEOUS CHONDRITES; ACCRETIONARY RIMS;
SOLAR NEBULA; CHONDRULES; METEORITE; BCAIS; EFREMOVKA; ORIGIN
AB The forsterite-bearing Type B (FoB) CAI SJ101 consists of three major structural units: (1) light patches of sector-zoned, poikilitic Al-rich clinopyroxene (Cpx) with numerous inclusions of small spine] grains and aggregates and subordinate amounts of Mg-rich melilite (Mel) and anorthite (An) (Sp-Cpx lithology), (2) dark sinuous bands of Al-rich clinopyroxene with large (up to similar to 300 x 60 mu m) poikilitically enclosed euhedral forsterite (Fo) crystals (Fo-Cpx lithology), and (3) the external Cpx-Sp-An rim overlying the entire inclusion. The two major lithologies are always separated by a transition zone of clinopyroxene poikilitically enclosing both forsterite and spinel. The patches of the Sp-Cpx lithology exhibit significant textural and mineralogical variability that is size-dependent. Small patches typically consist of Cpx and spinel with minor remnants of melilite and/or its alteration products. Large patches contain Mel-An-rich cores with either equigranular-ophitic-subophitic or 'lacy' textures reminiscent of those in Types B or C CAIs, respectively. All silicates poikilitically enclose numerous spinel grains of identical habit. Both melilite and anorthite gradually disappear toward the boundary with the Fo-Cpx lithology. Neither the evaporation mantle of Al-rich melilite typical of other FoBs nor the Wark-Lovering rim is present. Secondary minerals include grossular, monticellite, magnetite, and a few grains of wollastonite, andradite, and nepheline.
Being a rather typical FoB mineralogically and chemically, texturally SJ101 differs from other FoBs in displaying the nearly complete segregation of forsterite from spinel which occur only in the Fo-Cpx and Sp-Cpx lithologies, respectively. The complex, convoluted internal structure of SJ101 suggests that the coarse-grained Sp-An-Mel-Cpx cores and Fo-Cpx lithology represent the precursor materials of FoBs, proto-CAIs and Fo-rich accretionary rims. While the inferred chemistry and mineralogy of the Fo-rich rims are fairly typical, the high angstrom k content in SJ101 melilite (78.7-82.3 mol.%) implies that the SJ101 proto-CAIs represent a new type of CAIs that has not been sampled before. This type of CAIs might have formed by remelting of spinel-rich condensates.
The Group II REE pattern, slightly negative delta(29)Si and delta(25)Mg values, and nearly solar ratios of the major elements in the bulk SJ101 suggest that its precursors, proto-CAIs and Fo-rich rims, could have formed by a non-equilibrium condensation in a closed system of solar composition somewhat depleted in a super-refractory evaporation residue. The proposed formation scenario of SJ101 invokes a non-steady cooling and condensation of the nebular gas interrupted by at least two distinct melting episodes required to account for the igneous textures of the Mel-An-Cpx-rich cores (proto-CAIs) and the Fo-Cpx lithology. Published by Elsevier Ltd.
C1 [Petaev, Michail I.; Jacobsen, Stein B.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Petaev, MI (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM mpetaev@fas.harvard.edu
RI Jacobsen, Stein/B-1759-2013
FU NASA Cosmochemistry and Origins; DOE [DE-FG52-06NA26215]
FX We are very thankful to Dr. Ursula B. Marvin for donating the Allende
end piece in which SJ101 was found. Fruitful discussions with Glenn J.
MacPherson and Alexander N. Krot as well as the review by Andrew M.
Davis helped to improve the manuscript and are greatly appreciated. We
thank Gang Yu for the ICP-MS measurements. This work was supported by
the NASA Cosmochemistry and Origins programs and the DOE Grant
DE-FG52-06NA26215.
NR 35
TC 10
Z9 10
U1 1
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2009
VL 73
IS 17
BP 5100
EP 5114
DI 10.1016/j.gca.2008.10.045
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 484LX
UT WOS:000269047700009
ER
PT J
AU Peckmann, J
Birgel, D
Kiel, S
AF Peckmann, Joern
Birgel, Daniel
Kiel, Steffen
TI Molecular fossils reveal fluid composition and flow intensity at a
Cretaceous seep
SO GEOLOGY
LA English
DT Article
ID ANAEROBIC METHANE OXIDATION; COLD SEEPS; MICROBIAL COMMUNITIES;
HYDROCARBON-SEEP; HYDROTHERMAL VENT; CONVERGENT MARGIN; LIPID BIOMARKER;
BLACK-SEA; SEDIMENTS; PATTERNS
AB An isolated Hauterivian marine limestone from the Crimean Peninsula containing masses of articulated specimens of the dimerelloid brachiopod Peregrinella has previously been interpreted to represent a hydrocarbon-seep deposit. In order to constrain the intensity of seepage and the composition of fl uids, we investigated the lipid biomarker inventory of this seep limestone. The dominant biomarkers are (13)C-depleted isoprenoids including tail-to-tail linked pentamethylicosane (delta(13)C value: -108 parts per thousand), representing molecular fossils of methanotrophic archaea. This observation reveals that the seepage fl uids contained methane. Because the seep carbonates have been found to be only moderately (13)C-depleted (delta(13)C values as low as -14 parts per thousand), a signifi cant contribution from a less (13)C-depleted carbon source than methane, probably marine carbonate, is apparent. Such a degree of admixture of marine carbonate is typical for seep limestones resulting from low fl ow rates. The observed biomarker pattern with the prominent occurrence of biphytanes, but lacking crocetane, reveals that the methanotrophic archaea at the Hauterivian seep site were similar to archaea of the ANME-1 cluster. Archaea of this cluster are known to be able to cope with lower methane concentrations than ANME-2 archaea; therefore ANME-1 archaea are better adapted to low seepage rates and diffusive fl ow. The Peregrinella limestone contains only a small amount of early diagenetic cement. Based on a comparison with biomarker patterns of other ancient seep deposits, it is apparent that diffusive seepage typically results in limestones with little cement, whereas advective, more intense seepage appears to favor cement precipitation. If applied with caution, this supposed relationship can be used as a fi rst approximation of seepage intensity.
C1 [Peckmann, Joern; Birgel, Daniel] Univ Bremen, MARUM Zentrum Marine Umweltwissensch, D-28334 Bremen, Germany.
[Kiel, Steffen] Univ Kiel, Inst Geowissensch, D-24118 Kiel, Germany.
[Kiel, Steffen] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Peckmann, J (reprint author), Univ Bremen, MARUM Zentrum Marine Umweltwissensch, D-28334 Bremen, Germany.
EM peckmann@uni-bremen.de
RI Kiel, Steffen/C-3150-2009;
OI Kiel, Steffen/0000-0001-6281-100X; Peckmann, Jorn/0000-0002-8572-0060
FU Deutsche Forschungsgemeinschaft; European Commission
[MEIF-CT-2005-515420]
FX We thank Olga and Vitaliy Anistratenko (Kiev, Ukraine) for their help
during fieldwork and Sarah Janoschek (Bremen, Germany) for lipid
extraction. Comments by Jim Goedert (Wauna, Washington, USA) and the two
Geology reviewers, Rich Pancost (Bristol, UK) and an anonymous referee,
helped to improve the manuscript. Financial support was provided by the
"Deutsche Forschungsgemeinschaft" through the DFG Excellence Cluster
MARUM, Bremen, and the European Commission through a Marie Curie
fellowship (MEIF-CT-2005-515420) to Steffen Kiel.
NR 37
TC 56
Z9 56
U1 2
U2 10
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD SEP
PY 2009
VL 37
IS 9
BP 847
EP 850
DI 10.1130/G25658A.1
PG 4
WC Geology
SC Geology
GA 494KP
UT WOS:000269812000023
ER
PT J
AU Zimbelman, JR
Irwin, RP
Williams, SH
Bunch, F
Valdez, A
Stevens, S
AF Zimbelman, James R.
Irwin, Rossman P., III
Williams, Steven H.
Bunch, Fred
Valdez, Andrew
Stevens, Scott
TI The rate of granule ripple movement on Earth and Mars
SO ICARUS
LA English
DT Article
DE Earth; Geological processes; Mars surface
ID GREAT-SAND-DUNES; AEOLIAN BEDFORMS; GUSEV CRATER; SALTATION; COLORADO
AB The rate of movement for 3- and 10-cm-high granule ripples was documented in September of 2006 at Great Sand Dunes National Park and Preserve during a particularly strong wind event. Impact creep induced by saltating sand caused 24 granules min(-1) to cross each cm of crest length during wind that averaged similar to 9 m s(-1) (at a height well above 1 m), which is substantially larger than the threshold for saltation of sand. Extension of this documented granule movement rate to Mars suggests that a 25-cm-high granule ripple should require from hundreds to thousands of Earth-years to move I cm under present atmospheric conditions. Published by Elsevier Inc.
C1 [Zimbelman, James R.; Irwin, Rossman P., III] Smithsonian Inst, CEPS, NASM, MRC 315, Washington, DC 20013 USA.
[Williams, Steven H.] Smithsonian Inst, Educ Div, NASM, MRC 305, Washington, DC 20013 USA.
[Bunch, Fred; Valdez, Andrew] Great Sand Dunes Natl Pk & Preserve, Mosca, CO 81146 USA.
[Stevens, Scott] Natl Climat Ctr, Asheville, NC 28801 USA.
RP Zimbelman, JR (reprint author), Smithsonian Inst, CEPS, NASM, MRC 315, Washington, DC 20013 USA.
EM zimbelmanj@si.edu
FU Great Sand Dunes National Park and Preserve; National Climatic Data
Center; NASA [NNG04GN88G]
FX The comments of Nathan Bridges and an anonymous reviewer were extremely
helpful in correcting and clarifying earlier versions of the manuscript.
We are grateful for the support of personnel from both the Great Sand
Dunes National Park and Preserve and the National Climatic Data Center.
This work was supported in part by research grant NNG04GN88G from the
Mars Data Analysis Program of NASA.
NR 42
TC 23
Z9 24
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP
PY 2009
VL 203
IS 1
BP 71
EP 76
DI 10.1016/j.icarus.2009.03.033
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 599HV
UT WOS:000277902900009
ER
PT J
AU Pisano, DA
AF Pisano, Dominick A.
TI Untitled REPLY
SO ISIS
LA English
DT Letter
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Pisano, DA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0021-1753
J9 ISIS
JI Isis
PD SEP
PY 2009
VL 100
IS 3
BP 627
EP 628
PG 3
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 511GA
UT WOS:000271150700012
ER
PT J
AU Henson, P
AF Henson, Pamela
TI Everyday Nature: Knowledge of the Natural World in Colonial New York.
SO ISIS
LA English
DT Book Review
C1 [Henson, Pamela] Smithsonian Inst Arch, Inst Hist Div, Washington, DC 20560 USA.
[Henson, Pamela] American Univ, Dept Hist, Washington, DC 20016 USA.
RP Henson, P (reprint author), Smithsonian Inst Arch, Inst Hist Div, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0021-1753
J9 ISIS
JI Isis
PD SEP
PY 2009
VL 100
IS 3
BP 655
EP 656
PG 3
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 511GA
UT WOS:000271150700040
ER
PT J
AU Finkbeiner, DP
Slatyer, TR
Weiner, N
Yavin, I
AF Finkbeiner, Douglas P.
Slatyer, Tracy R.
Weiner, Neal
Yavin, Itay
TI PAMELA, DAMA, INTEGRAL and signatures of metastable excited WIMPs
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter theory; dark matter experiments
ID MICROWAVE-ANISOTROPY-PROBE; RAY POSITRON FRACTION; DARK-MATTER;
EMISSION; COSMOLOGY; ELECTRONS; ENERGIES; LINE
AB Models of dark matter with similar to GeV scale force mediators provide attractive explanations of many high energy anomalies, including PAMELA, ATIC, and the WMAP haze. At the same time, by exploiting the similar to MeV scale excited states that are automatically present in such theories, these models naturally explain the DAMA/LIBRA and INTEGRAL signals through the inelastic dark matter (iDM) and exciting dark matter (XDM) scenarios, respectively. Interestingly, with only weak kinetic mixing to hypercharge to mediate decays, the lifetime of excited states with delta < 2m(electron) is longer than the age of the universe. The fractional relic abundance of these excited states depends on the temperature of kinetic de-coupling, but can be appreciable. There could easily be other mechanisms for rapid decay, but the consequences of such long-lived states are intriguing. We find that CDMS constrains the fractional relic population of similar to 100 keV states to be less than or similar to 10(-2), for a 1TeV WIMP with sigma(n) - 10(-40) cm(2). Upcoming searches at CDMS, as well as xenon, silicon, and argon targets, can push this limit significantly lower. We also consider the possibility that the DAMA excitation occurs from a metastable state into the XDM state, which decays via e(+)e(-) emission, which allows lighter states to explain the INTEGRAL signal due to the small kinetic energies required. Such models yield dramatic signals from down-scattering, with spectra peaking at high energies, sometimes as high as similar to 1MeV, well outside the usual search windows. Such signals would be visible at future Ar and Si experiments, and may be visible at Ge and Xe experiments, although gamma-rays associated with nuclear excitations would complicate the signal for these heavier targets. We also consider other XDM models involving similar to 500 keV metastable states, and find they can allow lighter WIMPs to explain INTEGRAL as well.
C1 [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Slatyer, Tracy R.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Weiner, Neal] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA.
[Yavin, Itay] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
RP Finkbeiner, DP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dfinkbeiner@cfa.harvard.edu; tslatyer@fas.harvard.edu;
neal.weiner@nyu.edu; iyavin@princeton.edu
FU NSF CAREER [PHY-0449818]; DOE [DE-FG02-06ER41417, DE-FG02-90ER40542];
NSF [PHY-0756966]
FX The authors thanks Blas Cabrera, Clifford Cheung, Rick Gaitskell,
Cristiano Galbiati, Lisa Goodenough, David E. Kaplan, Dan McKinsey,
Philip Schuster, Chris Stubbs, and Natalia Toro for useful discussions.
IY thanks Maxim Pospelov for early and provocative conversations on the
lifetimes of the excited states. The authors are especially indebted to
Nima Arkani-Hamed, in collaboration with whom the analysis on lifetimes
and freezeout was done, and who further provided many additional
insights. NW is supported by NSF CAREER grant PHY-0449818 and DOE OJI
grant # DE-FG02-06ER41417. IY is supported by the NSF under grant
PHY-0756966 and the DOE under grant DE-FG02-90ER40542.
NR 67
TC 30
Z9 30
U1 0
U2 2
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 SEP
PY 2009
IS 9
AR 037
DI 10.1088/1475-7516/2009/09/037
PG 22
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 505AN
UT WOS:000270659900037
ER
PT J
AU Smith, BD
AF Smith, Bruce D.
TI RESOURCE RESILIENCE, HUMAN NICHE CONSTRUCTION, AND THE LONG-TERM
SUSTAINABILITY OF PRE-COLUMBIAN SUBSISTENCE ECONOMIES IN THE MISSISSIPPI
RIVER VALLEY CORRIDOR
SO JOURNAL OF ETHNOBIOLOGY
LA English
DT Article
DE archaeology; Mississippi Valley; niche construction; resource resilience
ID FOREST; CONSERVATION; VEGETATION; NORTHWEST; FIRE; DOMESTICATION;
SETTLEMENT; IMPACT; CANADA; PLANT
AB In small-scale human societies, a variety of factors contribute to the sustainability of subsistence economies, including premeditated conservation measures, low human population levels and predation pressure, and limited technological capacity to adversely impact environments. Here I suggest that it is worthwhile to look beyond simple characterizations of small-scale societies as being "low impact" in terms of their limited population, predation, and technology. Instead, we should look more closely both at the degree to which primary prey species are resilient to human predation and at the extent to which the niche construction efforts of small-scale human societies may modify vegetation communities in ways that result in their capture of a larger percentage of an ecosystem's total biotic energy. The small-scale Pre-Columbian societies occupying the Mississippi River Valley provide a case study. Throughout the Middle and Late Holocene, indigenons groups in this major north-south environmental corridor relied for protein to a substantial degree on a set of animal species/species groups (White-tailed deer, fish, migratory waterfowl) that combined both a high biotic potential and relative immunity front over-exploitation. At the same time, they practiced an integrated overall strategy of restructuring vegetation communities in Ways that enhanced and expanded the habitats Of many important food sources.
C1 Natl Museum Nat Hist, Smithsonian Inst, Archaeobiol Program, Washington, DC 20560 USA.
RP Smith, BD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Archaeobiol Program, Washington, DC 20560 USA.
NR 62
TC 21
Z9 22
U1 0
U2 12
PU SOC ETHNOBIOLOGY
PI DENTON
PA UNIV NORTH TEXAS, DEPT GEOGRAPHY, 1155 UNION CIRCLE 305279, DENTON, TX
76203-5017 USA
SN 0278-0771
EI 2162-4496
J9 J ETHNOBIOL
JI J. Ethnobiol.
PD FAL-WIN
PY 2009
VL 29
IS 2
BP 167
EP 183
DI 10.2993/0278-0771-29.2.167
PG 17
WC Anthropology; Biology
SC Anthropology; Life Sciences & Biomedicine - Other Topics
GA 532DI
UT WOS:000272724400002
ER
PT J
AU Funk, WC
Cannatella, DC
Ryan, MJ
AF Funk, W. C.
Cannatella, D. C.
Ryan, M. J.
TI Genetic divergence is more tightly related to call variation than
landscape features in the Amazonian frogs Physalaemus petersi and
P-freibergi
SO JOURNAL OF EVOLUTIONARY BIOLOGY
LA English
DT Article
DE Amazon rainforest; behavioural isolation; genetic divergence; landscape
genetics; mating calls; microsatellites; Physalaemus; sexual selection;
speciation
ID PUSTULOSUS SPECIES GROUP; APPROXIMATE BAYESIAN COMPUTATION; ALLELE
FREQUENCY DATA; PARTIAL MANTEL TESTS; SEXUAL SELECTION; TUNGARA FROG;
POPULATION-STRUCTURE; MICROSATELLITE LOCI; AMBYSTOMA-TIGRINUM;
NEOTROPICAL FROG
AB Behavioural isolation from divergence in male advertisement calls and female preferences is hypothesized to cause genetic divergence and speciation in the Amazonian frogs Physalaemus petersi and P. freibergi, yet the importance of call variation and landscape features in genetic divergence is unresolved. We tested for correlations between genetic divergence at microsatellite loci and (1) call variables; and (2) landscape variables among 10 populations of these frogs. Genetic divergence was not correlated with geographical distance, rivers or elevation. There was a strong positive relationship, however, between genetic divergence and inter-population differences in one call variable, whine dominant frequency. Effective population sizes varied among sites (range = 15-846) and were often small, suggesting that genetic drift could influence call evolution. Evidence for fine-scale genetic structure within sites was also found. Our results support the hypothesis that behavioural isolation from divergence in male calls and female preferences causes genetic divergence and speciation.
C1 [Funk, W. C.; Cannatella, D. C.; Ryan, M. J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Cannatella, D. C.] Univ Texas Austin, Texas Nat Sci Ctr, Austin, TX 78712 USA.
[Ryan, M. J.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Funk, WC (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA.
EM chris.funk@colostate.edu
FU National Science Foundation [0 078 150]
FX We thank J. Espinoza and K. Ramirez (Instituto Nacional de Recursos
Naturales) and J.P. Barriga (Estacion Cientifica Yasuni) for assisting
with permits; A. Angulo, S. Padilla, and C. Torres-Gastello for
assistance in the field; K. Holle (Tambopata Research Center, Rainforest
Expeditions), P. Jenson and S. Madigosky (Amazon Conservancy for
Tropical Studies, Explorama Lodges), E. Schwartz (La Selva Lodge), and
D. Romo and K. Swing (Tiputini Biodiversity Station) for providing
accommodations in the field; J. Cordova and C. Aguilar (Museo de
Historia Natural, Universidad Nacional Mayor de San Marcos) and L.
Coloma, I. Tapia, and D. Almeida-Reinoso (Museo de Zoologia, Pontificia
Universidad Catolica del Ecuador) for providing curatorial assistance
and facilitating research in Peru and Ecuador respectively; L. Coloma
for providing tissue loans; B. Caudle for assistance in the laboratory;
U. Mueller for access to his sequencer; and X. Bernal and B. Dawson for
their assistance with call analysis. We also thank Kim Hoke for
providing comments on the manuscript. The Peruvian Instituto Nacional de
Recursos Naturales provided research and export permit numbers
08-C/C-2004-INRENA-IANP, 032-2004-INRENA-IFFS-DCB and 003 886-AG-INRENA;
the Ecuadorian Ministerio de Ambiente provided research and collection
permit number 004-IC-FAU-DNBAPVS/MA. We acknowledge the National Science
Foundation for funding from the IRCEB grant 0 078 150. This is
publication number 197 of the Yanayacu Natural History Research Group.
NR 99
TC 32
Z9 33
U1 6
U2 34
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1010-061X
J9 J EVOLUTION BIOL
JI J. Evol. Biol.
PD SEP
PY 2009
VL 22
IS 9
BP 1839
EP 1853
DI 10.1111/j.1420-9101.2009.01795.x
PG 15
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 485QH
UT WOS:000269138100005
PM 19583696
ER
PT J
AU Harasewych, MG
Oleinik, A
Zinsmeister, W
AF Harasewych, M. G.
Oleinik, Anton
Zinsmeister, William
TI THE CRETACEOUS AND PALEOCENE PLEUROTOMARIID (GASTROPODA: VETIGASTROPODA)
FAUNA OF SEYMOUR ISLAND, ANTARCTICA
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID BASIN; MADAGASCAR; EOCENE
AB Leptomaria antipodensis and Leptomaria hickmanae are described from the Upper Cretaceous [Maastrichtian] Lopez de Bertodano Formation, Seymour Island, and represent the first Mesozoic records of the family Pleurotomariidae from Antarctica. Leptomaria stillwelli, L. seymourensis, Conotomaria sobralensis and C. bayeri, from the Paleocene [Danian], Sobral Formation, Seymour Island, are described as new. Leptomaria larseniana (Wilckens, 1911) new combination, also from the Sobral Formation, is redescribed based on better-preserved material. The limited diversity of the pleurotomariid fauna of Seymour Island is more similar to that of the Late Cretaceous faunas of Australia and New Zealand in terms of the number of genera and species, than to the older, more diverse faunas of South America, southern India, or northwestern Madagascar, supporting the status of the Weddelian Province as a distinct biogeographic unit. The increase in the species richness of this fauna during the Danian may be due to the final fragmentation of Gondwana during this period.
C1 [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Oleinik, Anton] Florida Atlantic Univ, Dept Geosci, Boca Raton, FL 33431 USA.
[Zinsmeister, William] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA.
EM HARASEWYCH@si.edu; aoleinik@fau.edu; wjzins@purdue.edu
FU National Science Foundation [OPP 93-16034]
FX We are grateful to Dr. Rudiger Bieler for translating the original
description of Pleurotomaria larseniana. Thanks are due to Dr. Shiladri
Das for many informative discussions on the systematics and ecology of
Mesozoic Pleurotomariidae, particularly from the Kutch region of India.
We appreciate and gratefully acknowledge the many helpful comments and
insights of the referees, Dr. Steffen Kiel and Dr. Andrzei Kaim, as well
as of the editors, Dr. Peter Harries and Dr. Richard Lupia, which
markedly improved this paper. The field work on Seymour Island was
supported by the National Science Foundation grant OPP 93-16034.
NR 62
TC 6
Z9 6
U1 0
U2 2
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0022-3360
J9 J PALEONTOL
JI J. Paleontol.
PD SEP
PY 2009
VL 83
IS 5
BP 750
EP 766
DI 10.1666/09-004.1
PG 17
WC Paleontology
SC Paleontology
GA 499DX
UT WOS:000270198400006
ER
PT J
AU Suarez, W
Olson, SL
AF Suarez, William
Olson, Storrs L.
TI THE GENERIC POSITION OF MIRAQUILA TERRESTRIS CAMPBELL: ANOTHER ADDITION
TO THE BUTEOGALLINE RADIATION FROM THE PLESTOCENE OF PERU
SO JOURNAL OF RAPTOR RESEARCH
LA English
DT Article
DE Accipitridae; Amplibuteo; Buteogallus; South American raptors; Talara
tar pits
C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA.
[Suarez, William] Museo Nacl Hist Nat, Havana 10100, Cuba.
RP Suarez, W (reprint author), Museo Nacl Hist Nat, Obispo 61,Plaza Armas, Havana 10100, Cuba.
EM Olsons@si.edu
NR 9
TC 0
Z9 0
U1 0
U2 0
PU RAPTOR RESEARCH FOUNDATION INC
PI HASTINGS
PA 14377 117TH STREET SOUTH, HASTINGS, MN 55033 USA
SN 0892-1016
EI 2162-4569
J9 J RAPTOR RES
JI J. Raptor Res.
PD SEP
PY 2009
VL 43
IS 3
BP 249
EP 253
DI 10.3356/JRR-08-85.1
PG 5
WC Ornithology
SC Zoology
GA 497XU
UT WOS:000270099200008
ER
PT J
AU Wen, J
Xiang, QY
Qian, H
Li, JH
Wang, XQ
Ickert-Bond, SM
AF Wen, Jun
Xiang, Qiu-Yun (Jenny)
Qian, Hong
Li, Jianhua
Wang, Xiao-Quan
Ickert-Bond, Stefanie M.
TI Intercontinental and intracontinental biogeography-patterns and methods
SO JOURNAL OF SYSTEMATICS AND EVOLUTION
LA English
DT Editorial Material
ID DISPERSAL-VICARIANCE ANALYSIS; HISTORICAL BIOGEOGRAPHY; DIVERGENCE
TIMES; MOLECULAR EVOLUTION; NORTHERN-HEMISPHERE; PHYLOGENETIC TREES;
GEOGRAPHIC RANGE; ABSOLUTE RATES; LIKELIHOOD; EASTERN
C1 [Wen, Jun] Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA.
[Xiang, Qiu-Yun (Jenny)] N Carolina State Univ, Dept Plant Biol, Raleigh, NC 27695 USA.
[Qian, Hong] Illinois State Museum, Res & Collect Ctr, Springfield, IL 62703 USA.
[Li, Jianhua] Hope Coll, Dept Biol, Holland, MI 49423 USA.
[Wang, Xiao-Quan] Chinese Acad Sci, State Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum N Herbarium, Fairbanks, AK 99775 USA.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA.
RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, MRC 166, POB 37012, Washington, DC 20013 USA.
EM wenj@si.edu
RI Ickert-Bond, Stefanie/B-3216-2012
OI Ickert-Bond, Stefanie/0000-0001-8198-8898
NR 35
TC 6
Z9 7
U1 1
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1674-4918
EI 1759-6831
J9 J SYST EVOL
JI J. Syst. Evol.
PD SEP
PY 2009
VL 47
IS 5
SI SI
BP 327
EP 329
DI 10.1111/j.1759-6831.2009.00052.x
PG 3
WC Plant Sciences
SC Plant Sciences
GA 502RM
UT WOS:000270477800001
ER
PT J
AU Wen, J
Ickert-Bond, SM
AF Wen, Jun
Ickert-Bond, Stefanie M.
TI Evolution of the Madrean-Tethyan disjunctions and the North and South
American amphitropical disjunctions in plants
SO JOURNAL OF SYSTEMATICS AND EVOLUTION
LA English
DT Review
DE amphitropical disjunctions; biogeography; Madrean-Tethyan disjunctions;
Mediterranean disjuncts; North-South American disjunctions
ID LONG-DISTANCE DISPERSAL; NUCLEAR RIBOSOMAL DNA; CHLOROPLAST DNA;
HISTORICAL BIOGEOGRAPHY; EASTERN ASIA; MOLECULAR EVIDENCE;
PHYLOGENETIC-RELATIONSHIPS; TIQUILIA BORAGINACEAE; CHARACTER EVOLUTION;
VICARIANCE ANALYSIS
AB The present paper reviews advances in the study of two major intercontinental disjunct biogeographic patterns: (i) between Eurasian and western North American deserts with the Mediterranean climate (the Madrean-Tethyan disjunctions); and (ii) between the temperate regions of North and South America (the amphitropical disjunctions). Both disjunct patterns have multiple times of origin. The amphitropical disjunctions have largely resulted from long-distance dispersal, primarily from the Miocene to the Holocene, with available data indicating that most lineages dispersed from North to South America. Results of recent studies on the Mediterranean disjuncts between the deserts of Eurasia and western North America support the multiple modes of origin and are mostly consistent with hypotheses of long-distance dispersal and the North Atlantic migration. Axelrod's Madrean-Tethyan hypothesis, which implies vicariance between the two regions in the early Tertiary, has been favored by a few studies. The Beringian migration corridor for semiarid taxa is also supported in some cases.
C1 [Wen, Jun] Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, UA Museum N Herbarium, Fairbanks, AK 99775 USA.
[Ickert-Bond, Stefanie M.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA.
RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, MRC 166, POB 37012, Washington, DC 20013 USA.
EM wenj@si.edu
RI Ickert-Bond, Stefanie/B-3216-2012
OI Ickert-Bond, Stefanie/0000-0001-8198-8898
FU National Science Foundation [DEB 045573, DEB 0743474]; National Museum
of Natural History; Smithsonian Institution
FX The authors' work reported herein was supported, in part, by grants from
the National Science Foundation (DEB 045573 to Michael DILLON and Jun
WEN; and DEB 0743474 to Steve MANCHESTER and Jun WEN), and visiting
support for S. ICKERT-BOND from the National Museum of Natural History,
the Smithsonian Institution. The authors thank Jianhua LI (Hope College,
Michigan, USA), Tieyao TU (South China Botanical Garden, Guangzhou,
China), and Jenny XIANG (North Carolina State University, USA) for
constructive comments on the manuscript.
NR 131
TC 70
Z9 76
U1 3
U2 12
PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 1674-4918
J9 J SYST EVOL
JI J. Syst. Evol.
PD SEP
PY 2009
VL 47
IS 5
SI SI
BP 331
EP 348
DI 10.1111/j.1759-6831.2009.00054.x
PG 18
WC Plant Sciences
SC Plant Sciences
GA 502RM
UT WOS:000270477800002
ER
PT J
AU Nie, ZL
Sun, H
Meng, Y
Wen, J
AF Nie, Ze-Long
Sun, Hang
Meng, Ying
Wen, Jun
TI Phylogenetic analysis of Toxicodendron (Anacardiaceae) and its
biogeographic implications on the evolution of north temperate and
tropical intercontinental disjunctions
SO JOURNAL OF SYSTEMATICS AND EVOLUTION
LA English
DT Article
DE Anacardiaceae; biogeography; disjunction; eastern Asia; neotropics;
North America; phylogenetics; Toxicodendron
ID RHUS ANACARDIACEAE; SEQUENCE DATA; EASTERN ASIA; LAND-BRIDGE; AMERICA;
HEMISPHERE; DNA; TERTIARY; REGIONS; PSEUDOSMODINGIUM
AB Toxicodendron is a genus in the Rhus complex of Anacardiaceae with a disjunct distribution between eastern Asia and North America, extending to southeastern Asia and the neotropics. Nuclear (internal transcribed spacer, external transcribed spacer, and NIA-i3) and chloroplast (ndhF and trnL-F) sequences were used to construct phylogenetic relationships of Toxicodendron. Phylogenetic analysis of these data strongly support Toxicodendron as a monophyletic group distinct from other genera of the Rhus complex, and the phylogeny does not fully corroborate classification at the sectional level. Two temperate disjunct lineages were detected, one from section Toxicodendron and the other between the eastern North American Toxicodendron vernix and the eastern Asian Toxicodendron vernicifluum. Their divergence times were estimated to be 13.46 (7.95-19.42) and 7.53 (2.76-12.86) mya, respectively. The disjunction between section Griffithii (taxa from warm temperate to tropical Asia) and Toxicodendron striatum (from the neotropics) was supported and their divergence time was estimated to be 20.84 (11.16-30.52) mya in the early Miocene. Our biogeographic results and the paleontological data support the Bering land bridge as the most likely route to explain the temperate disjunctions, yet the tropical disjunction in Toxicodendron seems to be best explained by the North Atlantic land bridge hypothesis.
C1 [Nie, Ze-Long; Sun, Hang; Meng, Ying; Wen, Jun] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Peoples R China.
[Nie, Ze-Long] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China.
[Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Wen, Jun] Chinese Acad Sci, Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China.
RP Wen, J (reprint author), Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Peoples R China.
EM wenj@si.edu
FU National Basic Research Program of China [2007CB411601]; National
Natural Science Foundation of China [30625004, 40771073]; Yunnan Natural
Science Foundation [2008CC013]; John D. and Catherine T. MacArthur
Foundation; Laboratory of Analytical Biology of the National Museum of
Natural History, Smithsonian Institution, Washington DC, USA.
FX This study was supported by grants from the National Basic Research
Program of China (973 Program, grant no. 2007CB411601), the National
Natural Science Foundation of China (grant nos. 30625004 and 40771073 to
H. Sun), the Yunnan Natural Science Foundation (grant no. 2008CC013),
and the John D. and Catherine T. MacArthur Foundation (to J. Wen).
Laboratory work was carried out in and partially supported by the
Laboratory of Analytical Biology of the National Museum of Natural
History, Smithsonian Institution, Washington DC, USA. We thank Quentin
LUKE for his kind assistance in collecting samples in Kenya.
NR 82
TC 12
Z9 13
U1 3
U2 24
PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 1674-4918
J9 J SYST EVOL
JI J. Syst. Evol.
PD SEP
PY 2009
VL 47
IS 5
SI SI
BP 416
EP 430
DI 10.1111/j.1759-6831.2009.00045.x
PG 15
WC Plant Sciences
SC Plant Sciences
GA 502RM
UT WOS:000270477800007
ER
PT J
AU Dillon, MO
Tu, TY
Xie, L
Silvestre, VQ
Wen, J
AF Dillon, Michael O.
Tu, Tieyao
Xie, Lei
Quipuscoa Silvestre, Victor
Wen, Jun
TI Biogeographic diversification in Nolana (Solanaceae), a ubiquitous
member of the Atacama and Peruvian Deserts along the western coast of
South America
SO JOURNAL OF SYSTEMATICS AND EVOLUTION
LA English
DT Article
DE Atacama Desert; biogeography; chloroplast DNA; LEAFY second intron;
Nolana; Peruvian Desert; Solanaceae; South America
ID EL-NINO; PHYLOGENETIC ANALYSIS; MOLECULAR PHYLOGENY; NORTHERN CHILE;
SEQUENCES; CONVOLVULACEAE; NUCLEAR; FABACEAE; GENOME; DNA
AB The present paper reconstructs the biogeographic diversification for Nolana L.f. (Solanaceae), a genus of 89 endemic species largely restricted to fog-dependent desert lomas formations of coastal Peru and Chile. Previous efforts have reconstructed a phylogenetic estimate for Nolana using a combination of molecular markers. Herein, we expand on those results to examine hypotheses of biogeographic origins and diversification patterns. Nolana occupies habitats within a continuous coastal desert and forms a terrestrial archipelago of discrete "islands" unique in size, topography, and species composition. Each locality contains at least one Nolana species and many contain multiple species in sympatry. The genus has a Chilean origin, with the basal clades confined to Chile with wide geographic and ecological distributions. Peru contains two strongly supported clades, suggesting two introductions with subsequent radiation. A Chilean clade of shrubby, small-flowered species appears to have had its origins from the same ancestors of the second line that radiated in Peru and northern Chile. Nolana galapagensis is endemic to the Islas Galapagos, with origins traced to Peruvian taxa with a divergence time of 0.35 mya. Rates of diversification over the past 4.02 mya in Nolana, in one of the driest habitats on Earth, suggest rapid adaptive radiation in several clades. Success in Nolana may be attributed to characters that confer a competitive advantage in unpredictable and water-dependent environments, such as succulent leaf anatomy and ecophysiology, and the reproductive mericarp unique to Nolana. The processes affecting or shaping the biota of western South America are discussed.
C1 [Xie, Lei; Wen, Jun] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Peoples R China.
[Dillon, Michael O.] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA.
[Tu, Tieyao] Chinese Acad Sci, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Quipuscoa Silvestre, Victor] Univ Nacl San Agustin, Dept Bot, Arequipa, Peru.
[Wen, Jun] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Wen, J (reprint author), Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Peoples R China.
EM wenj@si.edu
FU National Science Foundation [DEB 0415573, DEB 9801297, DEB 8513205];
National Geographic Society; Pritzker Laboratory for Molecular
Systematics and Evolution of the Field Museum; National Museum of
Natural History; Smithsonian Institution
FX The curators and collection managers who facilitated examination of
their material are gratefully acknowledged. The collection of specimen
label data was supported, in part, by grants to MOD from the National
Science Foundation (DEB 0415573, DEB 9801297, DEB 8513205) and the
National Geographic Society. MOD and JW acknowledge the Pritzker
Laboratory for Molecular Systematics and Evolution of the Field Museum,
and the Laboratory of Analytical Biology of the National Museum of
Natural History, the Smithsonian Institution, for laboratory support.
The authors thank Lynn BOHS (Department of Biology, University of Utah,
Salt Lake City, UT, USA) for helpful discussions on the position of
Sclerophylax adnatifolia and the many people who provided material and
accompanied us during field studies. The authors thank Steffi
ICKERT-BOND (Department of Biology and Wildlife, University of Alaska,
Fairbanks, AL, USA) and Federico LUEBERT (Institut fur Biologie, Freie
Universitdt Berlin, Berlin, Germany) for valuable comments on the
original manuscript. Maximilian WEIGEND (Institut fur Biologie, Freie
Universitdt Berlin), Edgardo ORTIZ (Departamento de Botanica,
Universidad Nacional San Agustin, Arequipa, Peru) and Mario ZAPATA and
Segundo LEIVA (Museo de Historia Natural, Universidad Privada Antenor
Orrego, Trujillo, Peru) are given special recognition for their
collecting efforts. MOD thanks Federico LUEBERT and Patricio PLISCOFF
(Center for Advanced Studies in Ecology, Universidad de Chile, Santiago,
Chile) for discussions and sharing ecological data.
NR 74
TC 30
Z9 33
U1 1
U2 26
PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 1674-4918
J9 J SYST EVOL
JI J. Syst. Evol.
PD SEP
PY 2009
VL 47
IS 5
SI SI
BP 457
EP 476
DI 10.1111/j.1759-6831.2009.00040.x
PG 20
WC Plant Sciences
SC Plant Sciences
GA 502RM
UT WOS:000270477800010
ER
PT J
AU Pohl, CM
Hodgins, G
Speakman, RJ
Beaubien, HF
AF Pohl, Christie M.
Hodgins, Greg
Speakman, Robert J.
Beaubien, Harriet F.
TI THE EFFECT OF CYCLODODECANE ON CARBON-14 DATING OF ARCHAEOLOGICAL
MATERIALS
SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION
LA English
DT Article
AB The impact of cyclododecane on the carbon-14 dating of archaeological materials was investigated using accelerator mass spectrometry. Two conservation-grade and two laboratory-grade cyclododecane samples were determined to be radiocarbon-free, indicating that the chemical is synthesized from petroleum-derived, rather than modern hydrocarbon sources. Radiocarbon dating of modern and archaeological gourd rind samples that were treated with cyclododecane produced the same results as for untreated samples. While the study does not demonstrate that residues are absent from cyclododecane-treated artifacts, it showed that the stringent sample cleaning protocols specifically designed to remove both burial and laboratory contaminants were sufficient to reduce cyclododecane residues to levels that would not interfere with radiocarbon dating.
C1 [Hodgins, Greg] Univ Arizona, NSF Arizona AMS Lab, Tucson, AZ 85721 USA.
[Speakman, Robert J.; Beaubien, Harriet F.] Smithsonian Museum Conservat Inst, Museum Support Ctr, Suitland, MD 20746 USA.
RP Pohl, CM (reprint author), POB 82, Ctr Sandwich, NH 03227 USA.
EM ChristiePohl3@msn.com; ghodgins@physics.arizona.edu; speakmanj@si.edu;
beaubienh@si.edu
OI Speakman, Robert/0000-0003-2063-154X
NR 32
TC 0
Z9 0
U1 1
U2 3
PU MANEY PUBLISHING
PI LEEDS
PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND
SN 0197-1360
J9 J AM INST CONSERV
JI J. Am. Inst. Conserv.
PD FAL-WIN
PY 2009
VL 48
IS 3
BP 223
EP 233
PG 11
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA V29YI
UT WOS:000208783300003
ER
PT J
AU Redmond, NE
Mccormack, GP
AF Redmond, Niamh E.
Mccormack, Grace P.
TI Ribosomal internal transcribed spacer regions are not suitable for
intra- or inter-specific phylogeny reconstruction in haplosclerid
sponges (Porifera: Demospongiae)
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Porifera; Haplosclerida; Haliclona; Callyspongia; ITS-1; ITS-2
ID INTRAGENOMIC VARIATION; ORDER HAPLOSCLERIDA; PHYLUM PORIFERA; ITS2 RDNA;
18S RDNA; SEQUENCES; IDENTIFICATION; EMBRYOGENESIS; POPULATION;
AUSTRALIA
AB Sequences of the ribosomal internal transcribed spacer regions 1 and 2 (ITS-1 and ITS-2) were employed to investigate relationships between putatively very closely related species of marine haplosclerids and to investigate the species status of Haliclona cinerea. Results indicate that intra-genomic and intra-specific levels of diversity are equivalent, and sequences from multiple clones from a number of individuals of a single species could not be separated on phylogenetic trees. As a result, the ITS regions are not suitable markers for population level studies in marine haplosclerids. Sequences of these regions were highly species specific, and large differences were found between species. ITS sequences from three Callyspongia and three Haliclona species could not be aligned successfully and therefore this locus could not be used to investigate relationships between these putative close relatives. However, ITS sequences retrieved from one H. cinerea were very different from sequences generated from other H. cinerea individuals indicating that this species comprises more than one taxon.
C1 [Mccormack, Grace P.] Natl Univ Ireland Univ Coll Galway, Dept Zool, MRI, Mol Evolut & Systemat Lab, Galway, Ireland.
[Redmond, Niamh E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP Mccormack, GP (reprint author), Natl Univ Ireland Univ Coll Galway, Dept Zool, MRI, Mol Evolut & Systemat Lab, Galway, Ireland.
EM grace.mccormack@nuigalway.ie
FU Irish Research Council for Science, Engineering and Technology (IRCSET);
Millennium Research Fund, National University of Ireland, Galway
FX This work was funded by the Irish Research Council for Science,
Engineering and Technology (IRCSET) and the Millennium Research Fund,
National University of Ireland, Galway. The authors would like to thank
Marieke Koopmans, Bernard Picton, Rob van Soest and Michelle Kelly for
specimens. All experiments were carried out in Ireland and complied with
Irish law.
NR 27
TC 10
Z9 10
U1 2
U2 6
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD SEP
PY 2009
VL 89
IS 6
BP 1251
EP 1256
DI 10.1017/S0025315409000411
PG 6
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 498DX
UT WOS:000270118200022
ER
PT J
AU Cruz-Angon, A
Baena, ML
Greenberg, R
AF Cruz-Angon, Andrea
Baena, Martha L.
Greenberg, Russell
TI The contribution of epiphytes to the abundance and species richness of
canopy insects in a Mexican coffee plantation
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE bromeliads; canopy insects; community structure; Inga jinicuil; Mexico;
richness; shade coffee; vascular epiphytes
ID RAIN-FOREST TREES; COMMUNITY STRUCTURE; ARTHROPOD FAUNA; TROPICAL TREE;
LEAF DAMAGE; BODY LENGTH; DIVERSITY; BIODIVERSITY; ANT; COLEOPTERA
AB The abundance of epiphytes has been assumed to be important in explaining the high diversity of tropical canopy arthropods. In this study we assessed the possible role that the presence of epiphytes may have on the diversity and abundance of canopy insects in an experimental study conducted in a coffee plantation in Coatepec, Veracruz, Mexico. Epiphytes were removed from trees in one of two plots in two sites of the coffee plantation. In each plot we collected insects from three Inga jinicuil trees by knockdown insecticide fogging. Insects were sorted to morphospecies. counted and measured. Trees with epiphytes had significantly higher numbers of species and individuals and insects larger than 5 mm were also more species-rich and abundant in trees with epiphytes. The magnitude of the enhancement was surprisingly large with the epiphyte plot samples having on average 90% more individuals and 22% more species than plots without epiphytes. These differences were even greater for large (> 5 mm) insects (184%, and 113% respectively). Our results support the tenet that epiphytes provide valuable resources to arthropods, which we have illustrated for canopy insects in shade trees of coffee plantations.
C1 [Greenberg, Russell] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[Cruz-Angon, Andrea; Baena, Martha L.] Inst Ecol, AC Dept Ecol Func, Xalapa 91070, Veracruz, Mexico.
RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
EM greenbergr@si.edu
FU CONACYT [128767]; Smithsonian Institution; Departamento de Ecologia
Funciona; National Geographic Society
FX We thank A. Martinez-Fernandez for assistance with fieldwork. The
Martinez family and plantation manager R. Monge provided access to their
coffee plantation and permission to tree fogging. F. Becerril drew the
Inga iinicuil with epiphytes and trap setting for Figure 1. M. Ordano,
R. Munguia and C. Tejeda, gave statistical advice; J.G. Garcia-Franco,
Federico Escobar, S. Philpott, V. Rico-Gray, and M. Coro-Arizmendi
improved the manuscript with their comments and corrections. Funding to
ACA was provided by CONACYT (scholarship 128767), Smithsonian
Institution Fellowship 2002-2003, Departamento de Ecologia Funcional and
Laboratorio de Bioacustica of the Instituto de Ecologia and grants from
the National Geographic Society and Scholarly Studies Fund of the
Smithsonian Institution to RSG.
NR 73
TC 13
Z9 13
U1 2
U2 27
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD SEP
PY 2009
VL 25
BP 453
EP 463
DI 10.1017/S0266467409990125
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 486AV
UT WOS:000269168700001
ER
PT J
AU Valencia, R
Condit, R
Muller-Landau, HC
Hernandez, C
Navarrete, H
AF Valencia, Renato
Condit, Richard
Muller-Landau, Helene C.
Hernandez, Consuelo
Navarrete, Hugo
TI Dissecting biomass dynamics in a large Amazonian forest plot
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE Amazonia; biomass dynamics; climate change; Ecuador; growth; tropical
trees; Yasuni National Park
ID TROPICAL RAIN-FOREST; BRAZILIAN AMAZON; SECONDARY FORESTS; TREE; CARBON;
DISTRIBUTIONS; BALANCE; IMPACT
AB Above-ground biomass (AGB) is increasing inmost of the Amazon forests. One hypothesis is that forests are responding to widespread and intense human intervention prior to the European conquest (> 500 y ago). In this study we confront this hypothesis with changes in AGB over 6.3 y in a large western Amazonian forest plot (> 150 000 shrubs and trees and 1100 species with dbh >= 10 mm in 2 5 ha). We examined AGB flux in different habitats and across diameter classes. The forest lost small stems (4.6%), gained large trees (2.61%), and gained biomass (0.7%). The change in AGB stock was due entirely to this upward shift in size leading to more canopy trees and fewer saplings after just 6 y. Across habitats, the biggest increment in biomass was in the secondary-forest patch (3.4% y(-1)) which we know was cleared about 27 y ago, whereas mature forest on ridges and valleys had small increases (0.10%, and 0.09% y(-1), respectively). In both censuses. AGB stocks were > 50% higher on the ridge than in the valley while relative growth and mortality were higher in the valley. Mean wood specific gravity (WSG) decreased with increasing diameter class: WSG did not change much between censuses in mature forests and did not contribute to the change in AGB stocks. Our forest increased its standing biomass, but far less than the average reported for other Amazonian forests (i.e. 0.30 vs. 0.98 Mg ha(-1) y(-1)). We find no evidence to support the notion that this forest is recovering from long-past human intervention. Instead of a long-term recovery. we believe the forest changed in response to natural fluctuations of the environment (e.g. changes in precipitation, higher CO(2)). windstorms or other more recent events. The significant differences in AGB stocks between valley and ridge suggest that the terra firme forests are a mosaic of natural habitats, and that this mosaic is in part responsible for the variation in biomass stocks detected in Amazonian terra firme forests.
C1 [Valencia, Renato; Hernandez, Consuelo; Navarrete, Hugo] Pontificia Univ Catolica Ecuador, Lab Ecol Plantas & Herbario QCA, Escuela Ciencias Biol, Quito, Ecuador.
[Condit, Richard] Smithsonian Trop Res Inst, Global Forest Observ Network, Balboa, Ancon, Panama.
RP Valencia, R (reprint author), Pontificia Univ Catolica Ecuador, Lab Ecol Plantas & Herbario QCA, Escuela Ciencias Biol, Apartado 17-01-2184, Quito, Ecuador.
EM lrvalencia@puce.edu.ec
FU government of Ecuador; National Science Foundation [DEB-0090311,
DEB-9806828]; Mellon Foundation; Tupper Family Foundation; Smithsonian
Tropical Research Institute (STRI); Pontificia Universidad Catolica del
Ecuador (PUCE); STRI Latin American Senior Scholar Award
FX The Yasuni Forest Dynamics Plot (YFDP) was established with
contributions from many professional workers, students, field assistants
and volunteers; some of them have worked with us for over a decade. We
wish to thank Robin Foster, Alvaro Perez, Gorky Villa, Margot Bass,
Pablo Alvia and Katya Romoleroux for the taxonomic identifications:
Anelio Loor, Jairo Zambrano, Milton Zambrano, Gabriel Grefa, Jugalio
Suarez, Wilson Loor and Milton Pabon carefully mapped and measured
trees. Carolina Altamirano provided unpublished data on wood specific
gravity. Funding for the study plot was provided by the government of
Ecuador (Donaciones del impuesto a la Renta 2004-2006), the National
Science Foundation (grants DEB-0090311. and DEB-9806828); the Mellon
Foundation, the Tupper Family Foundation. and the Smithsonian Tropical
Research Institute (STRI). Pontificia Universidad Catolica del Ecuador
(PUCE) and, in particular, Dr Manuel Corrales Pascual and Dr Laura
Arcos, enthusiastically supported the project. We gratefully acknowledge
the support of a STRI Latin American Senior Scholar Award (August
2008-February 2009) to RV, which allowed him to focus on the present
publication, and HSBC Climate Partnership funding to H.M. RV thanks
Catalina, Julian, Martin and Sebastian for their support while he was
abroad. The Ecuadorian Ministerio del Ambiente granted permission for
our work in Yasuni National Park.
NR 25
TC 24
Z9 25
U1 1
U2 20
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD SEP
PY 2009
VL 25
BP 473
EP 482
DI 10.1017/S0266467409990095
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 486AV
UT WOS:000269168700003
ER
PT J
AU Wells, K
Corlett, RT
Lakim, MB
Kalko, EKV
Pfeiffer, M
AF Wells, Konstans
Corlett, Richard T.
Lakim, Maklarin B.
Kalko, Elisabeth K. V.
Pfeiffer, Martin
TI Seed consumption by small mammals from Borneo
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE frugivory; Muridae; seed dispersal; seed predation; South-East Asia;
Tupaiidae
ID TROPICAL RAIN-FOREST; PROECHIMYS-SEMISPINOSUS; NEOTROPICAL FOREST; SMALL
RODENTS; PREDATION; MALAYSIA; RECRUITMENT; DISPERSAL; REMOVAL; FRUGIVORY
C1 [Wells, Konstans; Kalko, Elisabeth K. V.; Pfeiffer, Martin] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
[Corlett, Richard T.] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Wells, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany.
EM konstans.wells@uni-ulm.de
RI Wells, Konstans/A-7232-2010; Corlett, Richard/G-1251-2011; Pfeiffer,
Martin/A-6989-2012;
OI Wells, Konstans/0000-0003-0377-2463; Corlett,
Richard/0000-0002-2508-9465
FU German Academic Exchange Service (DAAD)
FX We thank the Economic Planning Unit Malaysia for a research permit and
Sabah Parks, Yayasan Sabah and the Universiti Malaysia Sabah for cordial
support during fieldwork. The German Academic Exchange Service (DAAD)
provided financial support. We are particularly indebted to the local
people and staff at all forest sites for their friendly support and warm
hospitality. We thank two anonymous reviewers for comments that have
improved this paper.
NR 30
TC 6
Z9 7
U1 1
U2 17
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD SEP
PY 2009
VL 25
BP 555
EP 558
DI 10.1017/S0266467409990058
PN 5
PG 4
WC Ecology
SC Environmental Sciences & Ecology
GA 486AV
UT WOS:000269168700012
ER
PT J
AU Estrada, AH
Gerlach, TJ
Schmidt, MK
Siegal-Willott, JL
Atkins, AL
Van Gilder, J
Citino, SB
Padilla, LR
AF Estrada, Amara H.
Gerlach, Trevor J.
Schmidt, Mandi K.
Siegal-Willott, Jessica L.
Atkins, Adrienne L.
Van Gilder, James
Citino, Scott B.
Padilla, Luis R.
TI CARDIAC EVALUATION OF CLINICALLY HEALTHY CAPTIVE MANED WOLVES
(CHRYSOCYON BRACHYURUS)
SO JOURNAL OF ZOO AND WILDLIFE MEDICINE
LA English
DT Article
DE Chrysocyon brachyurus; maned wolf; cardiology; radiography;
echocardiography; electrocardiography
ID ANGIOSTRONGYLUS-VASORUM INFECTION; M-MODE ECHOCARDIOGRAPHY; ANTIGEN TEST
KITS; DIROFILARIA-IMMITIS; CANIS-LATRANS; DOGS; RECOMMENDATIONS;
GUIDELINES; GREYHOUND; STANDARDS
AB The objective of this project was to determine radiographic vertebral heart sizes and electrocardiographic (ECG) and echocardiographic measurements in healthy anesthetized maned wolves (Chrysocyon brachyurus). The wolves, housed at the White Oak Conservation and Smithsonian National Zoo Conservation and Research Centers, were being anesthetized for annual examinations. Cardiac auscultation, thoracic radiographs, a standard 6-lead ECG, and echocardiography were performed on the wolves while they were under general anesthesia. Thirteen maned wolves were evaluated: five males and eight females. Mean age was 6.4 +/- 4.4 years (range, 2-13 years). Mean weight was 26 +/- 2.95 kg (range, 22-32 kg). Low-grade systolic murmurs were auscultated in three of 13 maned wolves. Evaluation of ECGs revealed a sinus rhythm, with a QRS morphology, and mean electrical axis similar to domestic canines. Radiographic evaluation revealed a mean vertebral heart size of 8.27 +/- 0.48 (range, 7.9-8.6). In addition, the cardiac silhouette was seen to elongate, with an increase in sternal contact in older wolves. Echocardiography showed that mitral valve degenerative changes and insufficiency is likely common in older wolves. Visualization of physiologic regurgitation across the mitral and pulmonary valves was common in wolves of all ages. Left ventricular measurements were similar to those reported for healthy dogs, and several variables correlated well with body weight. Two wolves were found to have one to three heartworms in the right pulmonary artery, and degenerative mitral valve disease was determined in maned wolves older than 6 years of age. All of the wolves in this study were on heartworm preventative and tested negative for heartworm antigen at their annual examinations. The results of this study provide reference information for use in the cardiac evaluation of anesthetized maned wolves.
C1 [Estrada, Amara H.; Gerlach, Trevor J.; Schmidt, Mandi K.; Siegal-Willott, Jessica L.; Atkins, Adrienne L.; Van Gilder, James] Univ Florida, Coll Vet Med, Dept Small Anim Clin Sci, Gainesville, FL 32610 USA.
[Citino, Scott B.] White Oak Conservat Ctr, Yulee, FL 32097 USA.
[Padilla, Luis R.] Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA.
RP Estrada, AH (reprint author), Univ Florida, Coll Vet Med, Dept Small Anim Clin Sci, POB 100126, Gainesville, FL 32610 USA.
EM EstradaA@vetmed.ufl.edu
NR 37
TC 8
Z9 8
U1 0
U2 5
PU AMER ASSOC ZOO VETERINARIANS
PI YULEE
PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA
SN 1042-7260
J9 J ZOO WILDLIFE MED
JI J. Zoo Wildl. Med.
PD SEP
PY 2009
VL 40
IS 3
BP 478
EP 486
DI 10.1638/2008-0154.1
PG 9
WC Veterinary Sciences
SC Veterinary Sciences
GA 493IC
UT WOS:000269729000011
PM 19746863
ER
PT J
AU Geyer, LB
Lessios, H
AF Geyer, Laura B.
Lessios, H. A.
TI Lack of Character Displacement in the Male Recognition Molecule, Bindin,
in Altantic Sea Urchins of the Genus Echinometra
SO MOLECULAR BIOLOGY AND EVOLUTION
LA English
DT Article
DE molecular divergence; reinforcement; selection; sympatry; reproductive
character displacement; Echinometra; adaptive evolution
ID DETECTING POSITIVE SELECTION; CODON-SUBSTITUTION MODELS; ACROSOMAL SPERM
PROTEIN; GAMETE RECOGNITION; ADAPTIVE EVOLUTION; SEXUAL CONFLICT;
REPRODUCTIVE ISOLATION; NUCLEOTIDE-SEQUENCES; MITOCHONDRIAL-DNA; RAPID
EVOLUTION
AB Bindin, a protein involved in sea urchin sperm-egg recognition and adhesion, is under positive selection in genera with sympatric species but evolves neutrally in genera in which all species are allopatric. This pattern has led to suggestions that reinforcement may be the source of the observed selection. Reproductive character displacement, or increased divergence of reproductive characters in areas where closely related species overlap, is often a consequence of reinforcement and has been shown to be present in one Indo-Pacific species of the genus Echinometra. In the Atlantic species of the same genus, positive selection has been shown to act on bindin of Echinometra lucunter. To examine whether the source of this selection is reinforcement, we determined variation on the first exon of bindin in E. lucunter in the Caribbean, where it is sympatric with Echinometra viridis, and in the rest of the Atlantic, where E. viridis is absent. There was no differentiation between bindin sequences from the two geographic regions; similar levels of positive selection were found to be acting in both areas. The similarities were not due to gene flow; mitochondrial DNA from the two regions indicates that E. lucunter populations most likely originated in the Atlantic and have not exchanged genes with Caribbean populations for approximately 200,000 years. The lack of evidence of stronger selection on bindin of E. lucunter in areas of sympatry with its sister species suggests that the source of selection is not reinforcement. Processes acting within species, such as sexual selection, sperm competition, or sexual conflict, are more likely to be involved in the evolution of this molecule.
C1 [Geyer, Laura B.; Lessios, H. A.] Smithsonian Trop Res Inst, Naos Marine Labs, Panama City, Panama.
RP Geyer, LB (reprint author), Smithsonian Trop Res Inst, Naos Marine Labs, Panama City, Panama.
EM geyerl@si.edu
NR 82
TC 16
Z9 16
U1 1
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0737-4038
J9 MOL BIOL EVOL
JI Mol. Biol. Evol.
PD SEP
PY 2009
VL 26
IS 9
BP 2135
EP 2146
DI 10.1093/molbev/msp122
PG 12
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 483WG
UT WOS:000269001500018
PM 19561091
ER
PT J
AU Puillandre, N
Strong, EE
Bouchet, P
Boisselier, MC
Couloux, A
Samadi, S
AF Puillandre, N.
Strong, E. E.
Bouchet, P.
Boisselier, M. -C.
Couloux, A.
Samadi, S.
TI Identifying gastropod spawn from DNA barcodes: possible but not yet
practicable
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE Barcode of Life Database; DNA barcoding; egg capsules; GenBank;
Neogastropoda
ID IN-SITU HYBRIDIZATION; TURRIDS MOLLUSCA; EGG CAPSULES; WHOLE-LARVAE;
IDENTIFICATION; ENVIRONMENTS; CHARACTERS; DIVERSITY; TAXONOMY; SHELL
AB Identifying life stages of species with complex life histories is problematic as species are often only known and/or described from a single stage. DNA barcoding has been touted as an important tool for linking life-history stages of the same species. To test the current efficacy of DNA barcodes for identifying unknown mollusk life stages, 24 marine gastropod egg capsules were collected off the Philippines in deep water and sequenced for partial fragments of the COI, 16S and 12S mitochondrial genes. Two egg capsules of known shallow-water Mediterranean species were used to calibrate the method. These sequences were compared to those available in GenBank and the Barcode of Life Database ( BOLD). Using COI sequences alone, only a single Mediterranean egg capsule was identified to species, and a single Philippine egg capsule was identified tentatively to genus; all other COI sequences recovered matches between 76% and 90% with sequences from BOLD and GenBank. Similarity-based identification using all three markers confirmed the Mediterranean specimens' identifications. A phylogenetic approach was also implemented to confirm similarity-based identifications and provide a higher-taxonomic identification when species-level identifications were not possible. Comparison of available GenBank sequences to the diversity curve of a well-sampled coral reef habitat in New Caledonia highlights the poor taxonomic coverage achieved at present in existing genetic databases, emphasizing the need to develop DNA barcoding projects for megadiverse and often taxonomically challenging groups such as mollusks, to fully realize its potential as an identification and discovery tool.
C1 [Puillandre, N.; Boisselier, M. -C.; Samadi, S.] Univ Paris 06, CNRS, MNHN, IRD,UMR Systemat Adaptat Evolut 7138, F-75231 Paris 05, France.
[Strong, E. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Bouchet, P.] Museum Natl Hist Nat, F-75231 Paris 05, France.
[Couloux, A.] Ctr Natl Sequencage, GENOSCOPE, F-91000 Evry, France.
RP Puillandre, N (reprint author), Univ Paris 06, CNRS, MNHN, IRD,UMR Systemat Adaptat Evolut 7138, CP26,57 Rue Cuvier, F-75231 Paris 05, France.
EM puillandre@mnhn.fr
RI samadi, sarah/G-5011-2010;
OI Strong, Ellen/0000-0001-7181-4114
NR 46
TC 25
Z9 29
U1 3
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-098X
EI 1755-0998
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD SEP
PY 2009
VL 9
IS 5
BP 1311
EP 1321
DI 10.1111/j.1755-0998.2009.02576.x
PG 11
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 482AH
UT WOS:000268855000003
PM 21564902
ER
PT J
AU Draheim, H
Cui, M
Dick, CW
AF Draheim, Hope
Cui, Melissa
Dick, Christopher W.
TI Characterization of 14 microsatellite DNA markers for the tropical
forest tree Virola surinamensis (Rol.) Warb. (Myristicaceae)
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE Barro Colorado Island; gene flow; Panama; tropical forest; Virola
AB Fourteen microsatellite DNA markers were developed for studies of gene flow in the Neotropical rain forest tree Virola surinamensis. The loci were unlinked and polymorphic in a sample of 21 individuals, with two to 10 alleles per locus and observed heterozygosity ranging from 0.14 to 0.76. The overall exclusion probability (0.997) indicates high resolution for parentage-based analyses of gene flow.
C1 [Draheim, Hope; Cui, Melissa; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48108 USA.
[Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
RP Dick, CW (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 830 N Univ Ave, Ann Arbor, MI 48109 USA.
EM cwdick@umich.edu
RI Dick, Christopher/A-8744-2008
NR 10
TC 3
Z9 3
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD SEP
PY 2009
VL 9
IS 5
BP 1386
EP 1388
DI 10.1111/j.1755-0998.2009.02667.x
PG 5
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 482AH
UT WOS:000268855000015
PM 21564914
ER
PT J
AU Werner, N
Zhuravleva, I
Churazov, E
Simionescu, A
Allen, SW
Forman, W
Jones, C
Kaastra, JS
AF Werner, N.
Zhuravleva, I.
Churazov, E.
Simionescu, A.
Allen, S. W.
Forman, W.
Jones, C.
Kaastra, J. S.
TI Constraints on turbulent pressure in the X-ray haloes of giant
elliptical galaxies from resonant scattering
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE turbulence; galaxies: abundances; cooling flows; X-rays: galaxies;
X-rays: individual: NGC 4636; NGC 4649; NGC 5813; NGC 1404; NGC 4472
ID REFLECTION GRATING SPECTROMETER; BOARD XMM-NEWTON; DEEP CHANDRA
OBSERVATION; PERSEUS CLUSTER; CENTAURUS CLUSTER; GAS MOTIONS; DARK
ENERGY; PROFILES; CORE; SPECTROSCOPY
AB The dense cores of X-ray emitting gaseous haloes of large elliptical galaxies with temperatures kT less than or similar to 0.8 keV show two prominent Fe xvii emission features, which provide a sensitive diagnostic tool to measure the effects of resonant scattering. We present here high-resolution spectra of five bright nearby elliptical galaxies, obtained with the reflection grating spectrometers (RGS) on the XMM-Newton satellite. The spectra for the cores of four of the galaxies show the Fe xvii line at 15.01 A being suppressed by resonant scattering. The data for NGC 4636 in particular allow the effects of resonant scattering to be studied in detail and to prove that the 15.01 A line is suppressed only in the dense core and not in the surrounding regions. Using deprojected density and temperature profiles for this galaxy obtained with the Chandra satellite, we model the radial intensity profiles of the strongest resonance lines, accounting for the effects of resonant scattering, for different values of the characteristic turbulent velocity. Comparing the model to the data, we find that the isotropic turbulent velocities on spatial scales smaller than approximate to 1 kpc are less than 100 km s(-1) and the turbulent pressure support in the galaxy core is smaller than 5 per cent of the thermal pressure at the 90 per cent confidence level, and less than 20 per cent at 95 per cent confidence. Neglecting the effects of resonant scattering in spectral fitting of the inner 2 kpc core of NGC 4636 will lead to underestimates of the chemical abundances of Fe and O by similar to 10-20 per cent.
C1 [Zhuravleva, I.; Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Churazov, E.] Moscow Space Res Inst, IKI, Moscow 117810, Russia.
[Forman, W.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Simionescu, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kaastra, J. S.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J. S.] Univ Utrecht, Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands.
EM norbertw@stanford.edu
RI Churazov, Eugene/A-7783-2013
FU DFG [CH389/3-2]; Chandra grant [AR7-8007X]; ESA member states; USA
(NASA; US Department of Energy [DE-AC02-76SF00515]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Postdoctoral Fellowship Award Number
PF8-90056 issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics and Space Administration under contract
NAS8-03060. The work of EC is supported by the DFG grant CH389/3-2. SWA
acknowledges support from Chandra grant AR7-8007X. 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
the USA (NASA). This work was supported in part by the US Department of
Energy under contract number DE-AC02-76SF00515.
NR 41
TC 52
Z9 52
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2009
VL 398
IS 1
BP 23
EP 32
DI 10.1111/j.1365-2966.2009.14860.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 485PU
UT WOS:000269136800020
ER
PT J
AU Governato, F
Brook, CB
Brooks, AM
Mayer, L
Willman, B
Jonsson, P
Stilp, AM
Pope, L
Christensen, C
Wadsley, J
Quinn, T
AF Governato, F.
Brook, C. B.
Brooks, A. M.
Mayer, L.
Willman, B.
Jonsson, P.
Stilp, A. M.
Pope, L.
Christensen, C.
Wadsley, J.
Quinn, T.
TI Forming a large disc galaxy from a z < 1 major merger
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: N-Body simulations; galaxies: evolution; galaxies: formation;
galaxies: interactions
ID MASS-METALLICITY RELATION; COLD DARK-MATTER; INTEGRAL-FIELD
SPECTROSCOPY; DIGITAL SKY SURVEY; STAR-FORMATION; STELLAR MASS;
LUMINOSITY FUNCTIONS; HIERARCHICAL-MODELS; RADIATIVE-TRANSFER;
ANGULAR-MOMENTUM
AB Using high-resolution SPH simulations in a fully cosmological Lambda cold dark matter context, we study the formation of a bright disc-dominated galaxy that originates from a 'wet' major merger at z = 0.8. The progenitors of the disc galaxy are themselves disc galaxies that formed from early major mergers between galaxies with blue colours. A substantial thin stellar disc grows rapidly following the last major merger and the present-day properties of the final remnant are typical of early-type spiral galaxies, with an i-band bulge-to-disc ratio similar to 0.65, a disc scalelength of 7.2 kpc, g - r = 0.5 mag, an H i linewidth (W(20)/2) of 238 km s(-1) and total magnitude i = -22.4. The key ingredients for the formation of a dominant stellar disc component after a major merger are (i) substantial and rapid accretion of gas through cold flows followed at late times by cooling of gas from the hot phase, (ii) supernova feedback that is able to partially suppress star formation during mergers and (iii) relative fading of the spheroidal component. The gas fraction of the progenitors' discs does not exceed 25 per cent at z < 3, emphasizing that the continuous supply of gas from the local environment plays a major role in the regrowth of discs and in keeping the galaxies blue. The results of this simulation alleviate the problem posed for the existence of disc galaxies by the high likelihood of interactions and mergers for galaxy-sized haloes at relatively low z.
C1 [Governato, F.; Brook, C. B.; Brooks, A. M.; Stilp, A. M.; Pope, L.; Christensen, C.; Quinn, T.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Brooks, A. M.] CALTECH, Pasadena, CA 91125 USA.
[Mayer, L.] Univ Zurich, Zurich, Switzerland.
[Mayer, L.] ETH, Zurich, Switzerland.
[Willman, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Willman, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Jonsson, P.] Univ Calif Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Wadsley, J.] Mac Master Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
RP Governato, F (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM fabio@astro.washington.edu
FU Theodore Dunham; HST [GO-1125]; NSF ITR [PHY-0205413]; NSF
[AST-0607819]; NASA [ATP NNX08AG84G]; UK's Science & Technology
Facilities Council [ST/F002432/1]; Jet Propulsion Laboratory
[HST-AR-10678, 10958, 30183]
FX Simulations were run at ARSC, NASA AMES and Texas Supercomputing Center.
FG acknowledges support from a Theodore Dunham grant, HST GO-1125, NSF
ITR grant PHY-0205413 (also supporting TQ), NSF grant AST-0607819 and
NASA ATP NNX08AG84G. CBB acknowledges the support of UK's Science &
Technology Facilities Council (ST/F002432/1). PJ was supported by
programmes HST-AR-10678 and 10958 and by Spitzer Theory Grant 30183 from
the Jet Propulsion Laboratory. We acknowledge discussions with several
smart people, among them Avishai Dekel, Mark Fardal, James Bullock and
Phil Hopkins. FG and AMB acknowledge the hospitality of the Max Planck
Institute during the writing of this paper.
NR 73
TC 130
Z9 131
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2009
VL 398
IS 1
BP 312
EP 320
DI 10.1111/j.1365-2966.2009.15143.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 485PU
UT WOS:000269136800043
ER
PT J
AU Hopkins, PF
Hickox, R
Quataert, E
Hernquist, L
AF Hopkins, Philip F.
Hickox, Ryan
Quataert, Eliot
Hernquist, Lars
TI Are most low-luminosity active galactic nuclei really obscured?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: active; galaxies: evolution; quasars: general; cosmology:
theory
ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; ADVECTION-DOMINATED
ACCRETION; HUBBLE-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; BRIGHT
SERENDIPITOUS SURVEY; XMM-NEWTON OBSERVATIONS; SEYFERT 2 GALAXIES; X-RAY
LUMINOSITY; PHOTOMETRICALLY CLASSIFIED QUASARS
AB At low Eddington ratios ((m)over dot), two effects make it more difficult to detect certain active galactic nuclei (AGN) given a particular set of selection methods. First, even allowing for fixed accretion physics, at low (m)over dot AGN become less luminous relative to their hosts, diluting their emission; the magnitude of the dilution depends on host properties and, therefore, on luminosity and redshift. Secondly, low-(m)over dot systems are expected and observed to transition to a radiatively inefficient state, which changes the spectral energy distribution ( SED) shape and dramatically decreases the luminosity at optical through infrared (IR) wavelengths. The effects of dilution are unavoidable, while the precise changes in accretion physics at low (m)over dot are somewhat uncertain, but potentially very important for our understanding of AGN. These effects will have different implications for samples with different selection criteria, and generically lead to differences in the AGN populations recovered in observed samples, even at fixed bolometric luminosity and after correction for obscuration. Although the true Eddington ratio distribution may depend strongly on mass/luminosity, this will be seen only in surveys robust to dilution and radiative inefficiency, such as X-ray or narrow-line samples; by contrast, selection effects imply that AGN in optical samples will have uniformly high Eddington ratios, with little dependence on luminosity, even at low L-bol where the median 'true' (m)over dot less than or similar to 0.01. These same selection effects also imply that different selection criteria pick out systems with different hosts: as a result, the clustering of low- luminosity optical/IR sources will be weaker than that of X-ray sources, and optical/IR Seyferts will reside in more disc-dominated galaxies, while X-ray-selected Seyferts will be preferentially in early-type systems. Taken together, these effects can naturally explain longstanding, apparently contradictory claims in the literature regarding AGN Eddington ratio distributions, host populations and clustering. Finally, we show that if current observed Eddington ratio distributions are correct, a large fraction of low- luminosity AGN currently classified as 'obscured' are in fact radiatively diluted and/or radiatively inefficient, not obscured by gas or dust. This is equally true if X-ray hardness is used as a proxy for obscuration, since radiatively inefficient SEDs near (m)over dot similar to 0.01 are characteristically X-ray hard. These effects can explain most of the claimed luminosity/redshift dependence in the 'obscured' AGN population, with the true obscured fraction as low as similar to 20 per cent.
C1 [Hopkins, Philip F.; Quataert, Eliot] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hopkins, Philip F.; Quataert, Eliot] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[Hickox, Ryan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM phopkins@astro.berkeley.edu
FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690]; NASA ATP
[NAG5-12140, NAG5-13292, NAG5-13381, NNG06GI68G]; Miller Institute for
Basic Research in Science, University of California Berkeley; David and
Lucile Packard Foundation
FX We thank Paul Martini and Smita Mathur for helpful discussions. We also
thank the anonymous referee for valuable comments and suggestions. This
work was supported in part by NSF grants ACI 96-19019, AST 00-71019, AST
02-06299 and AST 03-07690, and NASA ATP grants NAG5-12140, NAG5-13292
and NAG5-13381. Support for PFH was provided by the Miller Institute for
Basic Research in Science, University of California Berkeley. EQ is
supported in part by NASA grant NNG06GI68G and the David and Lucile
Packard Foundation.
NR 189
TC 47
Z9 47
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 SEP 1
PY 2009
VL 398
IS 1
BP 333
EP 349
DI 10.1111/j.1365-2966.2009.15136.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 485PU
UT WOS:000269136800045
ER
PT J
AU Liu, A
Tegmark, M
Bowman, J
Hewitt, J
Zaldarriaga, M
AF Liu, Adrian
Tegmark, Max
Bowman, Judd
Hewitt, Jacqueline
Zaldarriaga, Matias
TI An improved method for 21-cm foreground removal
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; techniques: interferometric; early Universe;
radio lines: general
ID 21 CENTIMETER FLUCTUATIONS; HIGH REDSHIFTS; TOMOGRAPHY; REIONIZATION;
EPOCH
AB 21-cm tomography is expected to be difficult in part because of serious foreground contamination. Previous studies have found that line-of-sight approaches are capable of cleaning foregrounds to an acceptable level on large spatial scales, but not on small spatial scales. In this paper, we introduce a Fourier space formalism for describing the line-of-sight methods, and use it to introduce an improved new method for 21-cm foreground cleaning. Heuristically, this method involves fitting foregrounds in Fourier space using weighted polynomial fits, with each pixel weighted according to its information content. We show that the new method reproduces the old one on large angular scales, and gives marked improvements on small scales at essentially no extra computational cost.
C1 [Liu, Adrian; Tegmark, Max; Hewitt, Jacqueline] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Liu, Adrian; Tegmark, Max; Hewitt, Jacqueline] MIT, Kavli Inst, Cambridge, MA 02139 USA.
[Bowman, Judd] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA.
RP Liu, A (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM acliu@mit.edu
FU NSF [AST-0134999, AST-05-06556]; David and Lucile Packard Foundation and
the Research Corporation; NASA [NNG05GJ40G]
FX We wish to thank Mike Matejek, Miguel Morales, Leslie Rogers and
Christopher Williams for helpful comments. MT was supported by NSF
grants AST-0134999 and AST-05-06556 as well as fellowships from the
David and Lucile Packard Foundation and the Research Corporation. MZ was
supported by NASA NNG05GJ40G and NSF AST-05-06556 as well as the David
and Lucile Packard, Alfred P. Sloan and John D. and Catherine T.
MacArthur foundations.
NR 16
TC 67
Z9 67
U1 0
U2 5
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2009
VL 398
IS 1
BP 401
EP 406
DI 10.1111/j.1365-2966.2009.15156.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 485PU
UT WOS:000269136800052
ER
PT J
AU Kosnik, MA
Hua, Q
Kaufman, DS
Wust, RA
AF Kosnik, Matthew A.
Hua, Quan
Kaufman, Darrell S.
Wuest, Raphael A.
TI Taphonomic bias and time-averaging in tropical molluscan death
assemblages: differential shell half-lives in Great Barrier Reef
sediment
SO PALEOBIOLOGY
LA English
DT Article
ID RADIOCARBON AGE CALIBRATION; STRATIGRAPHIC DISORDER; IDENTIFYING
OUTLIERS; BODY-SIZE; PRESERVATION; DISSOLUTION; CARBONATE; ENVIRONMENTS;
RECORD; SEA
AB Radiocarbon-calibrated amino acid racemization ages of 428 individually dated shells representing four molluscan taxa are used to quantify time-averaging and shell half-lives with increasing burial depth in the shallow-water carbonate lagoon of Rib Reef, central Great Barrier Reef, Australia. The top 20 cm of sediment contains a distinct, essentially modern assemblage. Shells recovered at depths from 25 to 125 cm are age-homogeneous and significantly older than the surface layer. Taxon age distributions within sedimentary layers indicate that the top 125 cm of lagoonal sediment is thoroughly mixed on a sub-century scale. The age distributions and shell half-lives of four taxa (Ethalia, Natica, Tellina, and Turbo) are found to be largely distinct. Shell half-lives do not coincide with any single morphological characteristic thought to infer greater durability, but they are strongly related to a combined durability score based on shell density, thickness, and shape. These results illustrate the importance of bioturbation in tropical sedimentary environments, indicate that age estimates in this depositional setting are sensitive to taxon choice, and quantify a taxon-dependent bias in shell longevity and death assemblage formation.
C1 [Kosnik, Matthew A.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
[Hua, Quan] Australian Nucl Sci & Technol Org, Menai, NSW 2234, Australia.
[Kaufman, Darrell S.] No Arizona Univ, Dept Geol, Flagstaff, AZ 86011 USA.
[Wuest, Raphael A.] James Cook Univ, Sch Earth & Environm Sci, Townsville, Qld 4811, Australia.
RP Kosnik, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012,NHB MRC 121, Washington, DC 20013 USA.
EM mkosnik@alumni.uchicago.edu; qhx@ansto.gov.au; Darrell.Kaufman@nau.edu;
Raphael.Wust@jcu.edu.au
RI Kosnik, Matthew/G-2312-2010; Kaufman, Darrell/A-2471-2008
OI Kosnik, Matthew/0000-0001-5380-7041; Kaufman,
Darrell/0000-0002-7572-1414
FU Australian Institute of Nuclear Science and Engineering [05/098,
06/100]; Ian Potter Foundation; PADI Foundation [248]; James Cook
University Merit Research; National Science Foundation; Wilson
FX The author list is alphabetical following the lead author, and each
coauthor contributed time, thought, and effort to this paper. We thank
R. Gegg, G. Ewels, and M. LaBarbera for key contributions to the
sampling equipment and methodology; the divers who assisted with sample
collection (W. Beynon, N. Bigourdan, D. Feary, E. Graham, A. Kerswell,
J. Livingstone, J. Maddams, W. Robbins, A. Swaddling, and E. Walker);
the crew of the R/V Jantes Kirby (D. Battersby, M. O'Leary, and G.
Topping); the Tidal Unit of Maritime Safety Queensland for providing
tidal measurements and advice on water depth corrections; J. Bright and
C. Orem for generating the AAR data; S. Whittaker for assistance with
SEM imagery; J. Wingerath for preparing shell cross-sections; B. Boykins
for assistance with the acid dissolution experiment; T. Nickens for
assistance in accessing the Invertebrate Zoology collections at the
National Museum of Natural History; F. Harper, E. Hunt, S. Kidwell, R.
Lockwood, W. Ponder, and K. Wilson for helpful advice during the
creation of this manuscript; and K. Parsons-Hubbard, R. Krause, and S.
Kidwell for helpful and thoughtful reviews of the manuscript. This
research was funded by Australian Institute of Nuclear Science and
Engineering awards 05/098 and 06/100 (14C AMS analyses), Ian
Potter Foundation (sample collection), PADI Foundation research grant
248 (sample collection), James Cook University Merit Research Grant
(development of sampling methodology), National Science Foundation grant
EAR-0620455 (AAR analyses), and a Wilson grant (M.A.K. support).
NR 45
TC 39
Z9 39
U1 0
U2 11
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0094-8373
J9 PALEOBIOLOGY
JI Paleobiology
PD FAL
PY 2009
VL 35
IS 4
BP 565
EP 586
DI 10.1666/0094-8373-35.4.565
PG 22
WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Evolutionary Biology; Paleontology
GA 508TR
UT WOS:000270959800006
ER
PT J
AU Cottontail, VM
Wellinghausen, N
Kalko, EKV
AF Cottontail, V. M.
Wellinghausen, N.
Kalko, E. K. V.
TI Habitat fragmentation and haemoparasites in the common fruit bat,
Artibeus jamaicensis (Phyllostomidae) in a tropical lowland forest in
Panama
SO PARASITOLOGY
LA English
DT Article
DE Artibeus jamaicensis; habitat fragmentation; diversity; multi-host
parasite; haemoparasites; Trypanosoma; Litomosoides
ID LAND-BRIDGE ISLANDS; LYME-DISEASE RISK; INFECTIOUS-DISEASE; SUBGENUS
SCHIZOTRYPANUM; POPULATION-DYNAMICS; TRYPANOSOMA-CRUZI; CHAGAS-DISEASE;
HUMAN HEALTH; PALM TREES; ECOLOGY
AB Anthropogenic influence on ecosystems, Such as habitat fragmentation, impacts species diversity and interactions. There is growing evidence that degradation of habitats favours disease and hence affects ecosystem health. The prevalence of haemoparasites in the Common Fruit Bat (Artibeus jamaicensis) in a tropical. lowland forest in Panama was Studied. We assessed the relation of haemoparasite to the general condition of the animals and tested for possible association of haemoparasite prevalence to habitat fragmentation, with special focus on trypanosomes. Overall, a total of 250 A. jamaicensis sampled from fragmented sites, here man-made, forested islands in Lake Gatun, and sites in the adjacent, Continuous forest in and around the Barro Colorado Nature Monument were examined. Using microscopy and DNA-sequencing 2 dominant types of haemoparasite infections, trypanosomes and Litomosoides (Nematoda) were identified. Trypanosome prevalence was significantly higher in bats from forest fragments, than in bats captured in continuous forest. We attribute this to the loss of species richness in forest fragments and specific characteristics of the fragments favouring trypanosome transmission, in particular changes in vegetation cover. Interestingly, the effect of habitat fragmentation on the prevalence of trypanosomes as multi-host parasites Could not be observed in Litomosoides which probably has a higher host specificity and might be affected less by overall diversity loss.
C1 [Cottontail, V. M.; Kalko, E. K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
[Cottontail, V. M.; Wellinghausen, N.] Inst Med Microbiol & Hyg, D-89081 Ulm, Germany.
[Kalko, E. K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Cottontail, VM (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany.
EM veronika.cottontail@uni-ulm.de
FU Cusanuswerk; STRI trust funds
FX Financial support was provided by grants from the Cusanuswerk (V.M.C),
and the STRI trust funds (E. K. V. K.).
NR 77
TC 25
Z9 25
U1 2
U2 41
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0031-1820
J9 PARASITOLOGY
JI Parasitology
PD SEP
PY 2009
VL 136
IS 10
BP 1133
EP 1145
DI 10.1017/S0031182009990485
PG 13
WC Parasitology
SC Parasitology
GA 492GW
UT WOS:000269644100005
PM 19627629
ER
PT J
AU Franco, EFM
Violante-Gonzalez, J
Roche, DG
AF Mendoza Franco, Edgar F.
Violante-Gonzalez, Juan
Roche, Dominique G.
TI Interoceanic occurrence of species of Aristocleidus Mueller, 1936
(Monogenoidea: Dactylogyridae) parasitizing the gills of gerreid fishes
in the Neotropics
SO PARASITOLOGY RESEARCH
LA English
DT Article
ID MEXICO
AB During investigations of fish parasites in the Neotropics (including the state of Veracruz and the Yucatan Peninsula in the Gulf of Mexico, the Chautengo Lagoon on the Pacific coast of the state of Guerrero in Mexico, and Lake Gatun in the Panama Canal), three monogenoidean (Dactylogyridae) species were found parasitizing the gills of gerreids (Gerreidae): Aristocleidus hastatus Mueller, 1936, was recovered from Eugerres plumieri (Cuvier) and Diapterus auratus Ranzani in Veracruz, from D. auratus and Diapterus rhombeus (Cuvier) in Yucatan, from Eugerres brasilianus (Cuvier) in Panama (all new hosts and geographical records), and from D. peruvianus (Cuvier) and Gerres cinereus (Walbaum) in Guerrero; Aristocleidus lamothei Kritsky and Mendoza-Franco, 2008, was recovered from E. plumieri in Veracruz and from D. rhombeus in Yucatan (new hosts and geographical records), and Aristocleidus sp. was recovered from G. cinereus in Guerrero. Results from this study suggest that species of Aristocleidus exhibit wide host specificity within gerreid fishes and that geminate species within this parasite genus may have originated with the formation of the Isthmus of Panama (3.1 to 3.5 ma). Evidence is also presented suggesting the potential role of the Panama Canal as a passageway allowing the interoceanic dispersal of Aristocleidus species across the isthmus.
C1 [Mendoza Franco, Edgar F.] Acad Sci Czech Republic, Inst Parasitol, Ctr Biol, CR-37005 Ceske Budejovice, Czech Republic.
[Mendoza Franco, Edgar F.; Roche, Dominique G.] Smithsonian Trop Res Inst, Naos Isl Labs, Panama City, Panama.
[Violante-Gonzalez, Juan] Univ Autonoma Guerrero, Ecol Lab, Unidad Acad Ecol Marina, Acapulco 39390, Guerrero, Mexico.
[Roche, Dominique G.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
RP Franco, EFM (reprint author), Acad Sci Czech Republic, Inst Parasitol, Ctr Biol, Branisovska 31, CR-37005 Ceske Budejovice, Czech Republic.
EM oberon.men@gmail.com
RI Roche, Dominique/K-7426-2012;
OI Roche, Dominique/0000-0002-3326-864X
FU Center for Research and Advanced Studies (CINVESTAVIPN); Unidad
Academica de Ecolog a Marina at Universidad Autonoma de Guerrero (UAG),
Mexico; Consejo Nacional de Ciencia y Tecnolog a (CONACyT), Mexico
[C000/430/07-76029]; Institute of Parasitology of Ceske Budejovice in
the Czech Republic
FX We thank M. Hernandez-Santillana and D. Arceo of the Center for Research
and Advanced Studies (CINVESTAVIPN) and the students of the Unidad
Academica de Ecolog a Marina at Universidad Autonoma de Guerrero (UAG),
Mexico, for their invaluable help during fish sampling. We are also
grateful to D. R. Robertson (Smithsonian Tropical Research Institute)
for identifying the specimens of E. brasilianus and to Carlos
Mendoza-Palmero (Institute of Parasitology-ASCR, Ceske Budejovice) and
Mirza Ortega-Olivares and Jesus Montoya-Mendoza (Universidad Nacional
Autonoma de Mexico-UNAM) for providing parasite specimens from Veracruz.
D. C. Kritsky and M. E. Torchin provided useful comments on an earlier
version of this manuscript. The Consejo Nacional de Ciencia y Tecnolog a
(CONACyT), Mexico, awarded a postdoctoral fellowship (C000/430/07-76029)
to EFMF in support of his stay at the Institute of Parasitology of Ceske
Budejovice in the Czech Republic.
NR 11
TC 2
Z9 2
U1 0
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0932-0113
EI 1432-1955
J9 PARASITOL RES
JI Parasitol. Res.
PD SEP
PY 2009
VL 105
IS 3
BP 703
EP 708
DI 10.1007/s00436-009-1442-9
PG 6
WC Parasitology
SC Parasitology
GA 474WG
UT WOS:000268314400013
ER
PT J
AU Kozaki, T
Brady, SG
Scott, JG
AF Kozaki, Toshinori
Brady, Sean G.
Scott, Jeffrey G.
TI Frequencies and evolution of organophosphate insensitive
acetylcholinesterase alleles in laboratory and field populations of the
house fly, Musca domestica L.
SO PESTICIDE BIOCHEMISTRY AND PHYSIOLOGY
LA English
DT Article
DE Acetylcholinesterase; Polymorphism; Population; House fly; Genotyping
ID INSECTICIDE RESISTANCE; PERMETHRIN RESISTANCE; PYRETHROID RESISTANCE;
KNOCKDOWN RESISTANCE; SODIUM-CHANNELS; FLIES DIPTERA; NEW-YORK; STRAIN;
MUSCIDAE; GENE
AB Resistance to organophosphate (OP) and/or carbamate insecticides can be due to mutations in the acetylcholinesterase gene (Ace). Genotypes of house fly, Musca domestica L., Ace were determined in twelve laboratory maintained strains (originally from North America, Europe and Asia) and two field collected populations from New York and Florida. There were 15 Ace alleles found and 11 of the alleles coded for a susceptible form of the enzyme (i.e., V260, A316, G342 and F407). Three of the four resistance alleles were previously described, while one is new. Phylogenetic analysis of the alleles suggests multiple origins of the F407Y mutation and multiple origins of the G342A mutation that confer OP resistance. Genotyping of field collected house flies from New York and Florida populations revealed the presence of only one resistance allele, Acev10 (containing the non-synonymous mutations for A342 and Y407). All other alleles detected from the field-collected flies coded for a susceptible AChE. Thus, we were able to categorize individual flies as having homozygous susceptible (Ace(S)/Ace(S)), homozygous insensitive (Ace(I)/Ace(I) or Acev10/Acev10) or heterozygous AChE. The frequencies of Ace(S) and Ace(I) were not different between the NY2002 and FL2002 populations. Both populations were out of Castle-Hardy-Weinberg equilibrium, having an excess of Ace(S)/Ace(I) individuals and very few Ace(S)/Ace(S) individuals. Comparison of Ace, Vssc and CYP6D1 genotypes indicates individual house flies commonly have resistance alleles at multiple loci. Comparison of genotype data with bioassays, as well as the use of genotype data in resistance studies is discussed. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Kozaki, Toshinori; Scott, Jeffrey G.] Cornell Univ, Dept Entomol, Ithaca, NY 14850 USA.
[Kozaki, Toshinori] Natl Inst Agrobiol Sci, Tsukuba, Ibaraki 3058634, Japan.
[Brady, Sean G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Scott, JG (reprint author), Cornell Univ, Dept Entomol, Comstock Hall, Ithaca, NY 14850 USA.
EM JGS5@CORNELL.EDU
FU National Research Initiative of the USDA Cooperative State Research
Education and Extension Service [2005-35320-16226]; Daljit S. and Elaine
Sarkaria Professorship; National Science Foundation [EF-0431330]; Japan
Society for the Promotion of Science for Young Scientists [15-2384 (PD)]
FX We thank C. Leichter, J. Briddell, B. Kimmelblatt and J.-R. Gao for
technical assistance. The National Research Initiative of the USDA
Cooperative State Research Education and Extension Service, Grant #
2005-35320-16226, and the Daljit S. and Elaine Sarkaria Professorship
supported this project. S.G.B. is supported by National Science
Foundation Grant EF-0431330. Partial support for T.K was provided by a
research Fellowship from the Japan Society for the Promotion of Science
for Young Scientists (Grant # 15-2384 (PD)).
NR 44
TC 17
Z9 19
U1 3
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0048-3575
J9 PESTIC BIOCHEM PHYS
JI Pest. Biochem. Physiol.
PD SEP
PY 2009
VL 95
IS 1
BP 6
EP 11
DI 10.1016/j.pestbp.2009.04.015
PG 6
WC Biochemistry & Molecular Biology; Entomology; Physiology
SC Biochemistry & Molecular Biology; Entomology; Physiology
GA 474SD
UT WOS:000268303400002
ER
PT J
AU Litaker, RW
Vandersea, MW
Faust, MA
Kibler, SR
Chinain, M
Holmes, MJ
Holland, WC
Tester, PA
AF Litaker, R. Wayne
Vandersea, Mark W.
Faust, Maria A.
Kibler, Steven R.
Chinain, Mireille
Holmes, Michael J.
Holland, William C.
Tester, Patricia A.
TI Taxonomy of Gambierdiscus including four new species, Gambierdiscus
caribaeus, Gambierdiscus carolinianus, Gambierdiscus carpenteri and
Gambierdiscus ruetzleri (Gonyaulacales, Dinophyceae)
SO PHYCOLOGIA
LA English
DT Article
DE Ciguatera; D1-D3 LSU; D8-D10 LSU; Epitype; Evolution; Gambierdiscus
toxicus; ITS; Morphology; Phylogeny; rDNA; SSU
ID BENTHIC DINOFLAGELLATE; SP-NOV; CIGUATERA; DNA; VARIABILITY; TOXICUS
AB Gambierdiscus species produce toxins that cause ciguatera fish poisoning (CFP), the most common nonbacterial illness associated with fish consumption worldwide. Understanding the role that individual Gambierdiscus species play in causing CFP is hampered because the morphologically similar species in the genus are difficult to distinguish. Ambiguities in the description of the type species Gambierdiscus toxicus also exist. This paper presents detailed line drawings along with additional scanning electron microscopy (SEM) and light micrographs to more fully characterize the six known Gambierdiscus species in addition to describing four new species, Gambierdiscus caribaeus sp. nov., Gambierdiscus carolinianus sp. nov., Gambierdiscus carpenteri sp. nov., and Gambierdiscus ruetzleri sp. nov. All four of the new species are photosynthetic and epibenthic and have a Kofoidian plate formula of Po, 3', 7 '', 6C, 6 or 7S, 5''', 1 p, and 2 Establishment of these species is supported by both morphological differences and three independent phylogenetic analyses utilizing small-subunit, as well as D1-D3 and D8-D10 large-subunit rDNA gene sequences. During the course of this study it became apparent that the description of the type species, G. toxicus, included more than one species. Since no type material exists we propose that Fig. 1 in Adachi and Fukuyo (1979) be designated as the lectotype for this species and that the epithecal view of isolate GTT-91 shown in Fig. 1 from Chinain et al. (1999) be designated as the epitype. The GTT-91 isolate has been well characterized genetically and the original SEM stub of this isolate archived at the Smithsonian Institution has been re-examined to provide a more detailed morphological analysis of the epitype.
C1 [Litaker, R. Wayne; Vandersea, Mark W.; Kibler, Steven R.; Holland, William C.; Tester, Patricia A.] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA.
[Faust, Maria A.] Smithsonian Inst, Dept Bot, US Natl Herbarium, Suitland, MD 20746 USA.
[Chinain, Mireille] Inst Louis Malarde, Lab Microalgues Tox, Papeete, Tahiti, Fr Polynesia.
[Holmes, Michael J.] Natl Univ Singapore, Trop Marine Sci Inst, Singapore 119223, Singapore.
RP Litaker, RW (reprint author), NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA.
EM wayne.litaker@noaa.gov
FU Caribbean Coral Reef Ecosystem Program (CCRE); Smithsonian Institution;
Hunterdon Oceanographic Research Endowment
FX Dr. Robert A. Andersen provided helpful advice on the inclusion of
sequence data from type Cultures. Drs. Ojvind Moestrup, Paul Silva and
Antonio Calado provided advice on the epitype designation. Patrice Mason
provided helpful edits and suggestions. Special thanks to Alice Ilaya
Gedaria for culture of the G. yasumotoi cells and Elisabeth Laban for
technical assistance and Dr. Georgia L. Irby-Massie, Classical Studies
Department, College of William and Mary and Dan N. Nicolson, Department
of Botany, National Museum of Natural History (NMNH), Smithsonian
Institution for kindly providing the Latin translations. We thank Scott
Whittaker for skillful technical assistance and for providing access to
the Scanning Electron Microscope Laboratory, NMNH. We thank Dr. Klaus
RUitzler, NMNH, Smithsonian Institution for his long-term support of the
research program in Belize from which we have benefited greatly. Special
thanks to Michael Carpenter and Bertol Pfeiffer for logistic support.
Amy Nau provided technical editing. This research was partially
supported by a grant from the Caribbean Coral Reef Ecosystem Program
(CCRE), Smithsonian Institution. This is contribution number 858 of the
CCRE, Smithsonian Institution, supported in part by the Hunterdon
Oceanographic Research Endowment.
NR 38
TC 69
Z9 73
U1 1
U2 28
PU INT PHYCOLOGICAL SOC
PI LAWRENCE
PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0031-8884
J9 PHYCOLOGIA
JI Phycologia
PD SEP
PY 2009
VL 48
IS 5
BP 344
EP 390
DI 10.2216/07-15.1
PG 47
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 498SH
UT WOS:000270162900004
ER
PT J
AU Zhang, P
Dalgarno, A
Cote, R
AF Zhang, Peng
Dalgarno, Alex
Cote, Robin
TI Scattering of Yb and Yb+
SO PHYSICAL REVIEW A
LA English
DT Article
ID ULTRACOLD NEUTRAL PLASMA; FROZEN RYDBERG GAS
AB We calculate the cross sections for scattering of a neutral ytterbium atom with its positive ion at energies up to 30 eV. We identify peaks in the forward direction as arising from elastic collisions and those in the backward direction as from charge transfer. We show that the total cross section follows a semiclassical expression over a large range of energies and that the resonant charge transfer may be characterized by four energy regimes: an s-wave regime at ultralow energies, a modified Langevin regime at low energy, a Langevin regime at medium energy, and an "exchange" regime at high energy. We find large variations between the different isotopes for the two lowest-energy regimes and very little variation for the two highest-energy regimes. Our results are consistent with recent measurements.
C1 [Zhang, Peng; Dalgarno, Alex] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Cote, Robin] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
RP Zhang, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
FU Office of Basic Energy Science; Office of Science; (U.S.) Department of
Energy; National Science Foundation.
FX The authors wish to thank A. T. Grier and V. Vuletic for helpful
discussions. The research of A. D. and P. Z. was supported by the
Chemical Science, Geoscience, and Bioscience Division of the Office of
Basic Energy Science, Office of Science, (U.S.) Department of Energy and
of R. C. was supported by the National Science Foundation.
NR 28
TC 26
Z9 26
U1 1
U2 6
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD SEP
PY 2009
VL 80
IS 3
AR 030703
DI 10.1103/PhysRevA.80.030703
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 501LR
UT WOS:000270383900008
ER
PT J
AU Gordon, C
Pritchard, JR
AF Gordon, Christopher
Pritchard, Jonathan R.
TI Forecasted 21 cm constraints on compensated isocurvature perturbations
SO PHYSICAL REVIEW D
LA English
DT Article
ID COSMOLOGY; INFLATION; CREATION; UNIVERSE; GAS
AB A "compensated" isocurvature perturbation consists of an overdensity (or underdensity) in the cold dark matter which is completely cancelled out by a corresponding underdensity (or overdensity) in the baryons. Such a configuration may be generated by a curvaton model of inflation if the cold dark matter is created before curvaton decay and the baryon number is created by the curvaton decay (or vice versa). Compensated isocurvature perturbations, at the level producible by the curvaton model, have no observable effect on cosmic microwave background anisotropies or on galaxy surveys. They can be detected through their effect on the distribution of neutral hydrogen between redshifts 30-300 using 21 cm absorption observations. However, to obtain a good signal to noise ratio, very large observing arrays are needed. We estimate that a fast Fourier transform telescope would need a total collecting area of about 20 square kilometers to detect a curvaton generated compensated isocurvature perturbation at more than 5 sigma significance.
C1 [Gordon, Christopher] Univ Oxford, Beecroft Inst Particle Astrophys & Cosmol, Oxford OX1 2JD, England.
[Pritchard, Jonathan R.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA USA.
RP Gordon, C (reprint author), Univ Oxford, Beecroft Inst Particle Astrophys & Cosmol, Oxford OX1 2JD, England.
OI Gordon, Chris/0000-0003-4864-5150; Pritchard,
Jonathan/0000-0003-4127-5353
FU NASA [HST-HF-01211.01-A]
FX We thank Antony Lewis for helpful discussions. C. G. is supported by the
Beecroft Institute for Particle Astrophysics and Cosmology. J.R.P. is
supported by NASA through Hubble Grant No. HST-HF-01211.01-A awarded by
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., for NASA,
under Contract No. NAS 5-26555.
NR 41
TC 21
Z9 21
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD SEP
PY 2009
VL 80
IS 6
AR 063535
DI 10.1103/PhysRevD.80.063535
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 501ME
UT WOS:000270385200054
ER
PT J
AU McQuinn, M
Switzer, ER
AF McQuinn, Matthew
Switzer, Eric R.
TI Redshifted intergalactic He-3(+) 8.7 GHz hyperfine absorption
SO PHYSICAL REVIEW D
LA English
DT Article
ID ELECTRON-HYDROGEN COLLISIONS; EQUATION-OF-STATE; LY-ALPHA FOREST; HELIUM
REIONIZATION; FREQUENCY-RANGE; EARLY UNIVERSE; SPIN-EXCHANGE; 21-CM
LINE; RADIATION; SPECTRUM
AB Motivated by recent interest in redshifted 21 cm emission of intergalactic hydrogen, we investigate the 8.7 GHz S-2(1/2) F = 0 - 1 hyperfine transition of He-3(+). While the primordial abundance of He-3 relative to hydrogen is 10(-5), the hyperfine spontaneous decay rate is 680 times larger. Furthermore, the antenna temperature is much lower at the frequencies relevant for the He-3(+) transition compared to that of z > 6 21 cm emission. We find that the spin temperature of this 8.7 GHz line in the intergalactic medium is approximately the cosmic microwave background temperature, such that this transition is best observed in absorption against high-redshift, radio-bright quasars. We show that intergalactic 8.7 GHz absorption is a promising, unsaturated observable of the ionization history of intergalactic helium (for which He II -> He III reionization is believed to complete at z similar to 3) and of the primordial 3He abundance. Instruments must reach similar to 1 mu Jy RMS noise in bands of 1 MHz on a 1 Jy source to directly resolve this absorption. However, in combination with H I Ly alpha forest measurements, an instrument can statistically detect this absorption from z > 3 with 30 mu Jy RMS noise in 0.1 MHz spectral bands over 100 MHz, which may be within the reach of present instruments.
C1 [McQuinn, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Switzer, Eric R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
RP McQuinn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mmcquinn@cfa.harvard.edu; switzer@kicp.uchicago.edu
NR 81
TC 9
Z9 9
U1 3
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD SEP
PY 2009
VL 80
IS 6
AR 063010
DI 10.1103/PhysRevD.80.063010
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 501ME
UT WOS:000270385200019
ER
PT J
AU Angelier, F
Moe, B
Blanc, S
Chastel, O
AF Angelier, Frederic
Moe, Borge
Blanc, Samuel
Chastel, Olivier
TI What Factors Drive Prolactin and Corticosterone Responses to Stress in a
Long-Lived Bird Species (Snow Petrel Pagodroma nivea)?
SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY
LA English
DT Article
ID PITUITARY-ADRENAL AXIS; VASOACTIVE-INTESTINAL-PEPTIDE; BASE-LINE
CORTICOSTERONE; SEX-SPECIFIC PATTERNS; BREEDING SONG BIRD; REPRODUCTIVE
SUCCESS; BODY CONDITION; ADRENOCORTICAL-RESPONSE; PARENTAL BEHAVIOR;
CLUTCH SIZE
AB Life-history theory predicts that individuals should adapt their parental investment to the costs and benefits of the current reproductive effort. This could be achieved by modulating the hormonal stress response, which may shift energy investment away from reproduction and redirect it toward survival. In birds, this stress response consists of a release of corticosterone that may be accompanied by a decrease in circulating prolactin, a hormone involved in the regulation of parental care. We lack data on the modulation of the prolactin stress response. In this study, we tested the hypothesis that individuals should modulate their prolactin stress response according to the fitness value of the current reproductive effort relative to the fitness value of future reproduction. Specifically, we examined the influence of breeding status (failed breeders vs. incubating birds) and body condition on prolactin and corticosterone stress responses in a long-lived species, the snow petrel Pagodroma nivea. When facing stressors, incubating birds had higher prolactin levels than failed breeders. However, we found no effect of body condition on the prolactin stress response. The corticosterone stress response was modulated according to body condition but was not affected by breeding status. We also performed an experiment using injections of adrenocorticotropic hormone (ACTH) and found that the modulation of the corticosterone stress response was probably associated with a reduction in ACTH release by the pituitary and a decrease in adrenal sensitivity to ACTH. In addition, we examined whether prolactin and corticosterone secretion were functionally linked. We found that these two hormonal stress responses were not correlated. Moreover, injection of ACTH did not affect prolactin levels, demonstrating that short-term variations in prolactin levels are not governed directly or indirectly by ACTH release. Thus, we suggest that the corticosterone and prolactin responses to short-term stressors are independent and may therefore mediate some specific components of parental investment in breeding birds. With mounting evidence, we suggest that examining both corticosterone and prolactin stress responses could be relevant to parental investment in vertebrates.
C1 [Angelier, Frederic] Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[Angelier, Frederic; Blanc, Samuel; Chastel, Olivier] CNRS, Ctr Etudes Biol Chize, F-79360 Villiers En Bois, Deux Serves, France.
[Moe, Borge] Norwegian Univ Sci & Technol, Dept Biol, NO-7491 Trondheim, Norway.
[Moe, Borge] Norwegian Inst Nat Res, Div Arctic Ecol, NO-9296 Tromso, Norway.
RP Angelier, F (reprint author), Smithsonian Inst, Smithsonian Migratory Bird Ctr, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM angelierf@si.edu
RI Moe, Borge/P-2946-2015
OI Moe, Borge/0000-0002-2306-1899
FU Institut Paul Emile Victor; Centre National de la Recherche
Scientifique/Region Poitou-Charentes
FX This study was supported financially by the Institut Paul Emile Victor
(IPEV Programme 109). F. A. was supported by a grant from the Centre
National de la Recherche Scientifique/Region Poitou-Charentes. We are
grateful to Dr. A. F. Parlow for kindly providing us with a chicken kit
(bAFP 4444BQ) for prolactin assays. We are indebted to G. Bouteloup and
S. Jenouvrier for their assistance in the field and to R. L. Holberton
for advice on methodology. We thank B. Ballentine, who gave helpful
comments and improved the English of the original version of this
manuscript. At the Centre d'Etudes Biologiques de Chize, we thank S.
Dano, A. Lacroix, and C. Trouve for their excellent technical assistance
in corticosterone and prolactin assays.
NR 95
TC 23
Z9 23
U1 0
U2 13
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 1522-2152
J9 PHYSIOL BIOCHEM ZOOL
JI Physiol. Biochem. Zool.
PD SEP-OCT
PY 2009
VL 82
IS 5
BP 590
EP 602
DI 10.1086/603634
PG 13
WC Physiology; Zoology
SC Physiology; Zoology
GA 493MS
UT WOS:000269741700018
PM 19642948
ER
PT J
AU Deming, D
Seager, S
Winn, J
Miller-Ricci, E
Clampin, M
Lindler, D
Greene, T
Charbonneau, D
Laughlin, G
Ricker, G
Latham, D
Ennico, K
AF Deming, D.
Seager, S.
Winn, J.
Miller-Ricci, E.
Clampin, M.
Lindler, D.
Greene, T.
Charbonneau, D.
Laughlin, G.
Ricker, G.
Latham, D.
Ennico, K.
TI Discovery and Characterization of Transiting Super Earths Using an
All-Sky Transit Survey and Follow-up by the James Webb Space Telescope
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID EXOPLANET HD 189733B; EXTRASOLAR PLANET; TRANSMISSION SPECTRUM;
INFRARED-EMISSION; L-DWARFS; ATMOSPHERE; SEARCH; MODEL; PHOTOMETRY; JWST
AB Doppler and transit surveys are finding extrasolar planets of ever smaller mass and radius, and are now sampling the domain of super Earths (1-3R(circle plus)). Recent results from the Doppler surveys suggest that discovery of a transiting super Earth in the habitable zone of a lower main sequence star may be possible. We evaluate the prospects for an all-sky transit survey targeted to the brightest stars, that would find the most favorable cases for photometric and spectroscopic characterization using the James Webb Space Telescope (JWST). We use the proposed Transiting Exoplanet Survey Satellite (TESS) as representative of an all-sky survey. We couple the simulated TESS yield to a sensitivity model for the MIRI and NIRSpec instruments on JWST. Our sensitivity model includes all currently known and anticipated sources of random and systematic error for these instruments. We focus on the TESS planets with radii between those of Earth and Neptune. Our simulations consider secondary eclipse filter photometry using JWST/MIRI, comparing the 11 and 15 mu m bands to measure CO(2) absorption in super Earths, as well as JWST/NIRSpec spectroscopy of water absorption from 1.7-3.0 mu m, and CO(2) absorption at 4.3 mu m. We find that JWST will be capable of characterizing dozens of TESS super Earths with temperatures above the habitable range, using both MIRI and NIRspec. We project that TESS will discover about eight nearby habitable transiting super Earths, all orbiting lower-main-sequence stars. The principal sources of uncertainty in the prospective JWST characterization of habitable super Earths are super-Earth frequency and the nature of super-Earth atmospheres. Based on our estimates of these uncertainties, we project that JWST will be able to measure the temperature and identify molecular absorptions (water, CO(2)) in one to four nearby habitable TESS super Earths orbiting lower-main-sequence stars.
C1 [Deming, D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Seager, S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Seager, S.; Winn, J.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, J.; Ricker, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Miller-Ricci, E.; Charbonneau, D.; Latham, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Clampin, M.] NASA, Goddard Space Flight Ctr, Exoplanet & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Lindler, D.] NASA, Goddard Space Flight Ctr, Sigma Sci Corp, Greenbelt, MD 20771 USA.
[Greene, T.; Ennico, K.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Laughlin, G.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RI Clampin, mark/D-2738-2012; Ennico, Kimberly/L-9606-2014
FU JWST
FX T. Greene and M. Clampin gratefully acknowledge support from the JWST
Project. We thank J. Valenti for sending us his exoPTF White Paper, and
Lisa Kaltenegger for an advance copy of her ApJ paper. We are grateful
to Tilak Hewagama for a clarifying discussion on simulation of JWST
pointing jitter, and to the referee for helpful comments that
significantly improved the manuscript.
NR 60
TC 103
Z9 103
U1 2
U2 10
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2009
VL 121
IS 883
BP 952
EP 967
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 486WV
UT WOS:000269232300003
ER
PT J
AU Arnoldi, MJ
AF Arnoldi, Mary Jo
TI African Art and the Colonial Encounter: Inventing a Global Commodity
SO RESEARCH IN AFRICAN LITERATURES
LA English
DT Book Review
C1 [Arnoldi, Mary Jo] Smithsonian Inst, Washington, DC 20560 USA.
RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
EM ARNOLDIM@SI.EDU
NR 1
TC 0
Z9 0
U1 0
U2 0
PU INDIANA UNIV PRESS
PI BLOOMINGTON
PA 601 N MORTON STREET, BLOOMINGTON, IN 47404-3797 USA
SN 0034-5210
J9 RES AFR LITERATURES
JI Res. Afr. Lit.
PD FAL
PY 2009
VL 40
IS 3
BP 246
EP 247
PG 2
WC Literature, African, Australian, Canadian
SC Literature
GA 470DI
UT WOS:000267954300023
ER
PT J
AU Ma, B
Meng, KL
Pan, J
Huang, JS
Feng, LL
AF Ma, Bin
Meng, Ke-Lai
Pan, Jun
Huang, Jia-Sheng
Feng, Long-Long
TI Clustering of K-band selected local galaxies
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE galaxies: statistics; infrared: galaxies; cosmology: large-scale
structure of universe
ID DIGITAL SKY SURVEY; PAIRWISE VELOCITY DISPERSION; LARGE-SCALE STRUCTURE;
LUMINOSITY DEPENDENCE; REDSHIFT SURVEY; DEEP FIELD; UNIVERSE; MODELS;
SAMPLE; EVOLUTION
AB We present a detailed clustering analysis of a large K-band selected local galaxy sample, which is constructed from the 2MASS and the SDSS and consists of 82486 galaxies with 10 < K < 13.5 and 0.01 < z < 0.1. The two-point correlation function of the magnitude-limited sample in real space at small scales is well described by the power law xi(r) = (r/6.44 +/- 0.23)(-1.81) (+/-) (0.02). The pairwise velocity dispersion is derived from the anisotropic two-point correlation function and we find the dispersion sigma(12) = 685 +/- 17 km s(-1) if scale invariance is assumed, which is larger than values measured in the optical bands of the selected galaxy samples. We further investigate the dependence of the two-point correlation function and the sigma(12) on the g-r color and the K-band luminosity, and obtain similar results to previous works in optical bands. Comparing a mock galaxy sample with our real data indicates that the semi-analytical model cannot mimic the sigma(12) in observation, although it can approximate the two-point correlation function within measurement uncertainties.
C1 [Ma, Bin; Meng, Ke-Lai; Pan, Jun; Feng, Long-Long] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Huang, Jia-Sheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Feng, Long-Long] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
RP Ma, B (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
EM mabin@pmo.ac.cn
FU National Natural Science Foundation of China [10643002, 10633040,
10873035, 10725314]; Ministry of Science & Technology of China
[2007CB815402]; Chinese 863 [2006AA01A125]
FX This work is funded by the National Natural Science Foundation of China
under grant Nos. 10643002, 10633040, 10873035, 10725314 and the Ministry
of Science & Technology of China through 973 grant No. 2007CB815402. We
thank Xi Kang for providing the mock galaxy catalog. The N-body
simulation was performed at the Shanghai Supercomputer Center by Weipeng
Lin under the financial support of the Chinese 863 project (No.
2006AA01A125). This publication makes use of data products from the Two
Micron All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation. This publication
also makes use of the Sloan Digital Sky Survey (SDSS). Funding for the
creation and distribution of the SDSS Archive has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Aeronautics and Space Administration, the National Science Foundation,
the US Department of Energy, the Japanese Monbukagakusho, and the Max
Planck Society. The SDSS Web site is http://ww.sdvs.orgl. The SDSS
Participating Institutions are the University of Chicago, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, the Johns
Hopkins University, the Max Planck Institut fur Astronomic, the Max
Planck Institut fur Astrophysik, New Mexico State University, Princeton
University, the United States Naval Observatory, and the University of
Washington. This publication also made use of NASA's Astrophysics Data
System Bibliographic Services.
NR 46
TC 3
Z9 3
U1 0
U2 3
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD SEP
PY 2009
VL 9
IS 9
BP 979
EP 992
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 501TC
UT WOS:000270404200004
ER
PT J
AU Wang, J
Labandeira, CC
Zhang, GF
Bek, J
Pfefferkorn, HW
AF Wang, Jun
Labandeira, Conrad C.
Zhang, Guangfu
Bek, Jiri
Pfefferkorn, Hermann W.
TI Permian Circulipuncturites discinisporis Labandeira, Wang, Zhang, Bek et
Pfefferkorn gen. et spec. nov (formerly Discinispora) from China, an
ichnotaxon of a punch-and-sucking insect on Noeggerathialean spores
SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY
LA English
DT Article
DE Discinispora; ichnotaxon; Circulipuncturites; insect damage;
Thysanoptera
ID DISCINITES-SINENSIS WANG; THRIPS THYSANOPTERA; POLLEN; PLANT; STROBILUS;
MOUTHPARTS
AB The generic name Discinispora Wang, Zhang, Bek et Pfefferkorn was originally created for spores with an operculum-like structure that were found in a permineralized Noeggerathialean cone. Subsequently it was observed that up to three round and smooth openings can occur in different positions on the surface of a single spore. In light of the new observations, the previous interpretation as an operculum cannot be sustained. An interpretation implicating insect punch-and-sucking activity was suggested for these round structures. This new interpretation makes it necessary to withdraw the original diagnosis and the taxon. The insect-inflicted damage now is assigned to the ichnotaxon Circulipuncturites discinisporis Labandeira, Wang, Zhang, Bek et Pfefferkorn under the rules of the ICZN, rather than those of the ICBN that typified the insect-amaged host-plant spore. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Wang, Jun] Chinese Acad Sci, State Key Lab Paleobiol & Stratig, Nanjing Inst Geol & Paleontol, Nanjing 210008, Peoples R China.
[Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Zhang, Guangfu] Nanjing Normal Univ, Inst Life Sci, Nanjing 210008, Peoples R China.
[Bek, Jiri] Acad Sci Czech Republic, Inst Geol, Prague 16500, Czech Republic.
[Pfefferkorn, Hermann W.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
RP Wang, J (reprint author), Chinese Acad Sci, State Key Lab Paleobiol & Stratig, Nanjing Inst Geol & Paleontol, Nanjing 210008, Peoples R China.
EM jun.wang@nigpas.ac.cn
RI Bek, Jiri/I-8755-2014
FU Chinese Academy of Sciences [KZCX2-YW-105]; National Natural Science
Foundation of China [40572008, 40621062]; Ministry of Science and
Technology of China [2006CB806400]; National Museum of Natural History
(NMNH); Smithsonian Institution, in Washington, D.C; Czech Republic
[IAA301110701]; Academy of Sciences, Prague [AVOZ30130516]
FX We thank a colleague who sent Wang Jun an e-mail message suggesting the
possibility that the operculum of the spores of Discinites sinensis
could be the result of insect activity. Wang Bo is acknowledged for his
kind help in the identification of the current insect damage through
internet. JW, GZ, JB and HWF received funding for this study from of the
Chinese Academy of Sciences (Project KZCX2-YW-105), the National Natural
Science Foundation of China (Grants 40572008 and 40621062), and the
major Basic Research Project (Grant 2006CB806400) of the Ministry of
Science and Technology of China. CCL received funding from the Associate
Director of Research and Science, National Museum of Natural History
(NMNH), Smithsonian Institution, in Washington, D.C. This is
contribution 170 of the Evolution of Terrestrial Ecosystems Program of
the NMNH. We acknowledge financial support from the Grant Agency of the
Czech Republic (IAA301110701) and the Research Program (AVOZ30130516) of
the Institute of Geology v.v.i., Academy of Sciences, Prague.
NR 50
TC 10
Z9 10
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0034-6667
J9 REV PALAEOBOT PALYNO
JI Rev. Palaeobot. Palynology
PD SEP
PY 2009
VL 156
IS 3-4
BP 277
EP 282
DI 10.1016/j.revpalbo.2009.03.006
PG 6
WC Plant Sciences; Paleontology
SC Plant Sciences; Paleontology
GA 513PN
UT WOS:000271335300003
ER
PT J
AU Prevec, R
Labandeira, CC
Neveling, J
Castaldo, RA
Looy, CV
Bamford, M
AF Prevec, Rose
Labandeira, Conrad C.
Neveling, Johann
Castaldo, Robert A.
Looy, Cindy V.
Bamford, Marion
TI Portrait of a Gondwanan ecosystem: A new late Permian fossil locality
from KwaZulu-Natal, South Africa
SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY
LA English
DT Review
DE Permian; Lopingian; South Africa; Karoo; Glossopteris flora; herbivory;
plant-insect interactions; palynology; palaeoecology
ID PLANT-INSECT ASSOCIATIONS; PRINCE-CHARLES-MOUNTAINS; PENNSYLVANIAN TREE
FERNS; LATE PALEOZOIC FLORAS; NORTH-CENTRAL TEXAS; TRIASSIC BOUNDARY;
KAROO BASIN; GLOSSOPTERIS FLORA; EARLY HISTORY; ANTARCTICA
AB The Clouston Farm locality, assigned to the Lopingian Epoch and occurring within the Normandien Formation of the northeastern Karoo Basin, provides evidence for a community of diverse vascular plants occupying riparian woodland. The depositional environment is interpreted as an abandoned trunk channel that preserved a megaflora in slack-water phases punctuated by overbank deposits from rare flood events. Of 9772 plant specimens tabulated from an unbiased census of all fragments greater than similar to 1 cm(2), there are 51 distinct organ morphotypes, including glossopterids, sphenopsids, and ferns, collectively represented as foliage, axes, fructifications, and dispersed seeds. Of the 11 most abundant morphotypes 10 are glossopterid morphotypes or variant subtypes, in addition to a sphenopsid. Glossopterid morphotype dominance also is reflected in the palynoflora. Palynological data indicate a Wuchiapingian age for the locality. A specimen of the dicynodont 'Oudenodon,' found in a nearby stratigraphically equivalent. outcrop, is attributable to the Dicynodon Assemblage Zone, assigned a younger Changhsingian age. A rich record of plant-insect associations demonstrates an elevated frequency of external foliage feeding by mandibulate insects and lower incidence of oviposition by palaeodictyopteroid and odonatopteroid taxa. Evidence for piercing-and-sucking and galling is rare. The most abundant plant taxon (glossopterid Morphotype C2a) is the most intensively herbivorized, overwhelmingly by external feeding and ovipositing insects. Insect damage on this host is beyond that predicted by floristic abundance alone. This specificity, and high herbivory levels on other glossopterid taxa, demonstrates extension of the Euramerican pattern toward the preferential targeting of pteridosperms. The Clouston Farm site provides a glimpse into a late Permian ecosystem of primary producers, herbivores, and insectivores-a prelude to the crisis that engulfed life at the end of the period. Published by Elsevier B.V.
C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Prevec, Rose; Bamford, Marion] Univ Witwatersrand, Bernard Price Inst Palaeontol, ZA-2050 Johannesburg, South Africa.
[Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Neveling, Johann] Council Geosci, ZA-0001 Pretoria, South Africa.
[Castaldo, Robert A.] Colby Coll, Dept Geol, Waterville, ME 04901 USA.
[Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
EM labandec@si.edu
FU National Science Foundation [EAR-0230024, EAR-0417317, DEB-640107,
DEB-0345750]; National Geographic Society [7623-04]; American
Philosophical Society, Walcott Fund; National Museum of Natural History
FX We are grateful to Dr. Hallie Sims of the University of Iowa for
providing initial guidance and funding for this project. We dedicate
this paper to the memory of Mr. David Green, who brought this locality
to our attention. Members of the Clouston family have explored this site
for decades and we are grateful for their enthusiastic support of this
work and their generosity in allowing us access to their property. This
research was supported in part by the National Science Foundation
(EAR-0230024) to H.J. Sims, M.K. Bamford, and C.C. Labandeira,
(EAR-0417317) to R.A. Gastaldo, as well as the Bernard Price Institute
for Palaeontology (University of the Witwatersrand), the Council for
Geosciences, and Colby College. Additional funding for C.C. Labandeira
was provided by the National Geographic Society (Grant 7623-04),
American Philosophical Society, Walcott Fund and Small Grants Program of
the National Museum of Natural History, and the Restricted Endowments
Fund of the Smithsonian Institution. H. J. Sims also was supported by
the National Science Foundation (DEB-640107), as was C.C. Labandeira
(DEB-0345750). Finnegan Marsh expertly rendered the figures into journal
quality versions. This is contribution 156 of the Evolution of
Terrestrial Ecosystems consortium at the National Museum of Natural
History, which also provided support to R. Prevec and C. V. Looy.
Lastly, we are grateful to H. Kerp and two anonymous reviewers for
constructive commentary that resulted in a significantly improved
manuscript.
NR 213
TC 56
Z9 57
U1 0
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0034-6667
EI 1879-0615
J9 REV PALAEOBOT PALYNO
JI Rev. Palaeobot. Palynology
PD SEP
PY 2009
VL 156
IS 3-4
BP 454
EP 493
DI 10.1016/j.revpalbo.2009.04.012
PG 40
WC Plant Sciences; Paleontology
SC Plant Sciences; Paleontology
GA 513PN
UT WOS:000271335300017
ER
PT J
AU Schwartz, MS
Sadler, PM
Sonnert, G
Tai, RH
AF Schwartz, Marc S.
Sadler, Philip M.
Sonnert, Gerhard
Tai, Robert H.
TI Depth Versus Breadth: How Content Coverage in High School Science
Courses Relates to Later Success in College Science Coursework
SO SCIENCE EDUCATION
LA English
DT Article
ID CURRICULUM; KNOWLEDGE; EDUCATION; INSTRUCTION; DILEMMAS; REFORM
AB This study relates the performance of college students in introductory science courses to the amount of content covered in their high school science courses. The sample includes 83 10 students in introductory biology, chemistry, or physics courses in 55 randomly chosen U.S. colleges and universities. Students who reported covering at least I major topic in depth, for a month or longer, in high school were found to earn higher grades in college science than did students who reported no coverage in depth. Students reporting breadth in their high school course, covering all major topics, did not appear to have any advantage in chemistry or physics and a significant disadvantage in biology. Care was taken to account for significant covariates: socioeconomic variables, English and mathematics proficiency, and rigor of their preparatory high science course. Alternative operationalizations of depth and breadth variables result in very similar findings. We conclude that teachers should use their judgment to reduce coverage in high school science courses and aim for mastery by extending at least I topic in depth over an extended period of time. (C) 2008 Wiley Periodicals, Inc. Sci Ed 93:798-826 2009
C1 [Schwartz, Marc S.] Univ Texas Arlington, Arlington, TX 76019 USA.
[Sadler, Philip M.; Sonnert, Gerhard] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA.
[Tai, Robert H.] Univ Virginia, Curry Sch Educ, Curriculum Instruct & Special Educ Dept, Charlottesville, VA 22904 USA.
RP Schwartz, MS (reprint author), Univ Texas Arlington, Arlington, TX 76019 USA.
EM schwarma@uta.edu
NR 75
TC 25
Z9 25
U1 1
U2 19
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0036-8326
J9 SCI EDUC
JI Sci. Educ.
PD SEP
PY 2009
VL 93
IS 5
BP 798
EP 826
DI 10.1002/sce.20328
PG 29
WC Education & Educational Research
SC Education & Educational Research
GA 483NM
UT WOS:000268973700002
ER
PT J
AU Potvin, G
Hazari, Z
Tai, RH
Sadler, PM
AF Potvin, Geoff
Hazari, Zahra
Tai, Robert H.
Sadler, Philip M.
TI Unraveling Bias From Student Evaluations of Their High School Science
Teachers
SO SCIENCE EDUCATION
LA English
DT Article
ID FEMALE COLLEGE-TEACHERS; WOMENS MATH PERFORMANCE; GENDER-DIFFERENCES;
STEREOTYPE THREAT; PERCEPTIONS; MOTIVATION; PROFESSORS; INTERESTS;
PHYSICS; VIEWS
AB In this Study, the evaluation of high school biology, chemistry, and physics teachers by their Students is examined according to the gender of the Student and the gender of the teacher. Female teachers are rated significantly lower than male teachers by male students in all three disciplines, whereas female students underrate female teachers only in physics. Interestingly, physics is also the field that suffers the greatest lack of females and has been criticized most for its androcentric culture. The gender bias in teacher ratings persists even when accounting for academic performance, classroom experiences, and family support. Furthermore, male and female teachers in each discipline appear equally effective at preparing their Students for future science study in college, Suggesting that students have a discipline-specific gender bias. Such a bias may negatively impact female Students and Contribute to the loss of females in science, technology, engineering, and mathematics fields. (C) 2009 Wiley Periodicals, Inc. Sci Ed 93:827-845. 2009
C1 [Potvin, Geoff; Hazari, Zahra] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC 29634 USA.
[Potvin, Geoff; Hazari, Zahra] Clemson Univ, Dept Math Sci, Clemson, SC 29634 USA.
[Tai, Robert H.] Univ Virginia, Curry Sch Educ, Charlottesville, VA 22904 USA.
[Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA.
RP Potvin, G (reprint author), Clemson Univ, Dept Engn & Sci Educ, Clemson, SC 29634 USA.
EM gpotvin@clemson.edu
NR 37
TC 10
Z9 10
U1 2
U2 11
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0036-8326
J9 SCI EDUC
JI Sci. Educ.
PD SEP
PY 2009
VL 93
IS 5
BP 827
EP 845
DI 10.1002/sce.20332
PG 19
WC Education & Educational Research
SC Education & Educational Research
GA 483NM
UT WOS:000268973700003
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI From the CASTLE Smithsonian 2.0
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD SEP
PY 2009
VL 40
IS 6
BP 18
EP 18
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 487UA
UT WOS:000269300800011
ER
PT J
AU Cernusak, LA
Winter, K
Aranda, J
Virgo, A
Garcia, M
AF Cernusak, Lucas A.
Winter, Klaus
Aranda, Jorge
Virgo, Aurelio
Garcia, Milton
TI Transpiration efficiency over an annual cycle, leaf gas exchange and
wood carbon isotope ratio of three tropical tree species
SO TREE PHYSIOLOGY
LA English
DT Article
DE Platymiscium pinnatum; stem-wood delta C-13; Swietenia macrophylla;
Tectona grandis; water-use efficiency
ID WATER-USE EFFICIENCY; WHOLE-PLANT WATER; ORGANIC-MATTER; BOUNDARY-LAYER;
FICUS-INSIPIDA; PIONEER TREE; ELEVATED CO2; FOREST TREE; C-3 PLANTS;
DISCRIMINATION
AB Variation in transpiration efficiency (TE) and its relationship with the stable carbon isotope ratio of wood was investigated in the saplings of three tropical tree species. Five individuals each of Platymiscium pinnatum (Jacq.) Dugand, Swietenia macrophylla King and Tectona grandis Linn. f. were grown individually in large (760 1) pots over 16 months in the Republic of Panama. Cumulative transpiration was determined by repeatedly weighing the pots with a pallet truck scale. Dry matter production was determined by destructive harvest. The TE, expressed as experiment-long dry matter production divided by cumulative water use, averaged 4.1, 4.3 and 2.9 g dry matter kg(-1) water for P. pinnatum, S. macrophylla and T. grandis, respectively. The TE of T. grandis was significantly lower than that of the other two species. Instantaneous measurements of the ratio of intercellular to ambient CO2 partial pressures (c(i)/c(a)), taken near the end of the experiment, explained 66% of variation in TE. Stomatal conductance was lower in S. macrophylla than in T. grandis, whereas P. pinnatum had similar stomatal conductance to T. grandis, but with a higher photosynthetic rate. Thus, c(i)/c(a) and TE appeared to vary in response to both stomatal conductance and photosynthetic capacity. Stem-wood delta C-13 varied over a relatively narrow range of just 2.2 parts per thousand, but still explained 28% of variation in TE. The results suggest that leaf-level processes largely determined variation among the three tropical tree species in whole-plant water-use efficiency integrated over a full annual cycle.
C1 [Cernusak, Lucas A.; Winter, Klaus; Aranda, Jorge; Virgo, Aurelio; Garcia, Milton] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Cernusak, LA (reprint author), Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia.
EM lucas.cernusak@cdu.edu.au
RI Cernusak, Lucas/A-6859-2011
OI Cernusak, Lucas/0000-0002-7575-5526
FU Smithsonian Tropical Research Institute; Australian Research Council
FX We thank Ben Turner and Dayana Agudo for assistance with carbon isotope
analyses. L. A. C. was supported by a Tupper Postdoctoral Fellowship
from the Smithsonian Tropical Research Institute and by an Australian
Postdoctoral Fellowship from the Australian Research Council.
NR 46
TC 12
Z9 12
U1 1
U2 15
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0829-318X
EI 1758-4469
J9 TREE PHYSIOL
JI Tree Physiol.
PD SEP
PY 2009
VL 29
IS 9
BP 1153
EP 1161
DI 10.1093/treephys/tpp052
PG 9
WC Forestry
SC Forestry
GA 486QB
UT WOS:000269211100007
PM 19661136
ER
PT J
AU Wilkinson, FA
AF Wilkinson, Fiona A.
TI OBSERVATIONS ON THE BREEDING BIOLOGY OF THE SILKY-TAILED NIGHTJAR
(CAPRIMULGUS SERICOCAUDATUS MENGELI)
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
AB I found 15 nests of the Silky-tailed Nightjar (Caprimulgus sericocaudatus mengeli) from 1994 to 2004 at Cocha Cashu Biological Station, Mann National Park, Peru. Females and mates shared incubation and brooding duties with females on the nest during the day and males on at night. Nest relief occurred between 0300-0600 and 1800-2100 hrs. Two-egg clutches were placed on bare ground or on leaf-litter in more mature strands of forest. The semi-precocial young were mobile within 24 hrs of hatching and remained in the area with an adult through the fledgling stage. Both males and females feigned injury during incubation and brooding if disturbed. Three nesting sites were used for 5 years and another for 10 years, suggesting strong site fidelity and possibly a strong pair bond among long-lived individuals.
C1 Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Wilkinson, FA (reprint author), Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM wilkinsf@si.edu
NR 32
TC 4
Z9 4
U1 1
U2 3
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
EI 1938-5447
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD SEP
PY 2009
VL 121
IS 3
BP 498
EP 505
DI 10.1676/05-103.1
PG 8
WC Ornithology
SC Zoology
GA 492TM
UT WOS:000269682500006
ER
PT J
AU Olson, SL
Reveal, JL
AF Olson, Storrs L.
Reveal, James L.
TI Nomenclatural History and a New Name for the Blue-winged Warbler (Aves:
Parulidae)
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
AB Linnaeus (1766) proposed Certhia pinus based on two different entities, the Blue-winged Warbler (Vermivora pinus) and the Pine Warbler (Dendroica pinus). The confusion was noted by Wilson (1808-1814) who restricted Latham's (1790) Sylvia pinus, based on C. pinus, to the Pine Warbler (in 1811) and proposed, as a new species (in 1810), S. solitaria, for the Blue-winged Warbler. Wilson's effective lectotypification, long ignored, following which Bonaparte (1824) unequivocally restricted C. pinus to the Pine Warbler, has resulted in misapplication of C. pinus. The correct name of the Pine Warbler should be Dendroica pinus (Linnaeus) and not D. pinus (Wilson) as in modern lists. Wilson's Sylvia solitaria is unfortunately preoccupied by Sylvia solitaria Lewin 1808 (= Origma solitaria, the Rockwarbler of Australia). A new scientific name is provided here for the Blue-winged Warbler because no other is available.
C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Reveal, James L.] Cornell Univ, Dept Plant Biol, Ithaca, NY 14853 USA.
RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA.
EM olsons@si.edu
NR 17
TC 5
Z9 6
U1 0
U2 3
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD SEP
PY 2009
VL 121
IS 3
BP 618
EP 620
DI 10.1676/09-003.1
PG 3
WC Ornithology
SC Zoology
GA 492TM
UT WOS:000269682500018
ER
PT J
AU Olson, SL
AF Olson, Storrs L.
TI Additional Data on the Occurrence of the Plantaris Muscle in the
Hawaiian Finches (Carduelinae: Drepanidini)
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
ID HONEYCREEPERS DREPANIDIDAE; APPENDAGE MYOLOGY; FRINGILLIDAE
AB New data are presented on the phylogenetically informative plantaris muscle in the Drepanidini. The primitive condition (presence) corroborates the basal placement of the creepers of the genera Oreomystis and Paroreomyza. The derived condition of the plantaris (absence) was found in the Hawaii Creeper (Loxops mana), previously considered by some to be congeneric with Oreomystis, and agrees with other evidence placing that species in Loxops. The Hawaii Akepa (L. coccineus), Anianiau (L. parvus), and Kauai Amakihi (L. stejnegeri) also lack the plantaris. This condition still appears to define a monophyletic group within the Drepanidini.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA.
EM olsons@si.edu
NR 16
TC 1
Z9 2
U1 1
U2 2
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
EI 1938-5447
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD SEP
PY 2009
VL 121
IS 3
BP 621
EP 623
DI 10.1676/08-175.1
PG 3
WC Ornithology
SC Zoology
GA 492TM
UT WOS:000269682500019
ER
PT J
AU Wong, MML
Fedy, BC
Wilson, S
Martin, KM
AF Wong, Mark M. L.
Fedy, Brad C.
Wilson, Scott
Martin, Kathy M.
TI Adoption in Rock and White-tailed Ptarmigan
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
ID INTRASPECIFIC NEST PARASITISM; BROOD AMALGAMATION; POULT ADOPTION;
GOOSE; YOUNG; ABANDONMENT; HYPOTHESES; SURVIVAL; CANADA; GROUSE
AB Reports of adoption in birds are widespread, but few studies report rates of adoption or possible mechanisms for this phenomenon, particularly in the Order Galliformes. We report incidents of adoption in Rock Ptarmigan (Lagopus muta) and White-tailed Ptarmigan (L. leucura) from two sites in western Canada. Adoption rates for White-tailed Ptarmigan on Vancouver Island, British Columbia, and the Ruby Ranges, Yukon Territory were 13% (n = 16 broods) and 4% (n = 27), respectively, while rates for Rock Ptarmigan were 14% (n = 29) in the Ruby Ranges. Low brood densities may result in lower rates of adoption for ptarmigan.
C1 [Wong, Mark M. L.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada.
[Fedy, Brad C.] US Geol Survey, Ft Collins Sci Ctr, Ft Collins, CO 80526 USA.
[Wilson, Scott] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
[Martin, Kathy M.] Univ British Columbia, Forest Sci Ctr, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada.
RP Wong, MML (reprint author), Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada.
EM mmwong1@ualberta.ca
OI Fedy, Bradley/0000-0003-3933-4043
FU Upland Birds Society; Northern Scientific Training Program; Natural
Sciences and Engineering Research Council (NSERC)
FX We thank Danielle Dagenais, Amy Wilson, Sabine Nouvet, and Alana Clason
for assistance in the field. We are also grateful to D. S. Hik, Andy and
Sian Williams, and Lance Goodwin for logistical support at Pika Camp and
the Arctic Institute of North America at Kluane Lake. Financial support
was provided by the Upland Birds Society, Northern Scientific Training
Program, and Natural Sciences and Engineering Research Council (NSERC)
grants to Kathy Martin, B. C. Fedy, and Scott Wilson,
NR 25
TC 5
Z9 5
U1 0
U2 7
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD SEP
PY 2009
VL 121
IS 3
BP 638
EP 641
DI 10.1676/08-029.1
PG 4
WC Ornithology
SC Zoology
GA 492TM
UT WOS:000269682500024
ER
PT J
AU Strong, EE
Kohler, F
AF Strong, Ellen E.
Koehler, Frank
TI Morphological and molecular analysis of 'Melania' jacqueti Dautzenberg
and Fischer, 1906: from anonymous orphan to critical basal offshoot of
the Semisulcospiridae (Gastropoda: Cerithioidea)
SO ZOOLOGICA SCRIPTA
LA English
DT Article
ID FRESH-WATER; PHYLOGENETIC TREES; PLEUROCERIDAE; PACHYCHILIDAE;
EVOLUTION; MOLLUSKS; DNA; SYSTEMATICS; VICARIANCE; SEQUENCES
AB Morphological and molecular studies have been inconclusive in assessing monophyly of the Pleuroceridae s.l and the affinity of western North American Juga to Asian members of the family currently grouped in the Semisulcospirinae. In part, this has been hampered by the rarity of anatomical accounts for Asian pleurocerids (s.l.). The present study provides a comprehensive anatomical description of 'Melania'jacqueti- a Vietnamese species of uncertain generic placement forgotten in the scientific literature for over 100 years. This investigation confirmed that 'Melania'jacqueti and Juga possess a number of features that differentiate them from eastern North American species, including features of the kidney, prostate and pallial oviduct. However, comparative data remain inadequate to allow phylogenetic analysis based on morphological data alone. Consequently, a data set of partial mitochondrial 16S ribosomal RNA gene sequences for 51 pleurocerids (s.l.) and five outgroups (Melanopsidae, Thiaridae), was assembled. Parsimony, Bayesian and Maximum Likelihood analyses are largely congruent and support monophyly of the Pleuroceridae s.l., and of two large clades: (i) a clade of eastern North American species, and (ii) an Asian-American clade with 'Melania'jacqueti as the critical basal offshoot, decisively anchoring Juga within the Semisulcospirinae as sister to all remaining Asian forms. Given the morphological disparity between these two clades, this result is consistent with restriction of the concept of Pleuroceridae s.s. to eastern North American species, and elevation of the Asian-American clade to the rank of family - the Semisulcospiridae. Examination of available genus-group names for Oriental semisulcospirids supports placement of 'Melania'jacqueti in the genus Hua. Molecular calibration of the basal split between Semisulcospiridae and Pleuroceridae suggests they diverged in the Cretaceous (approximately 90 million years ago). The origin and diversification of these clades are roughly coincident with the subdivision of Laurasia by epicontinental seas and the opening of the Atlantic basin, consistent with a primarily vicariant explanation for their modern biogeographical distributions modified by dispersal in Juga.
C1 [Koehler, Frank] Humboldt Univ, Museum Nat Kunde, D-10115 Berlin, Germany.
RP Strong, EE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA.
EM stronge@si.edu; Frank.Koehler@austmus.gov.au
RI Kohler, Frank/C-4853-2009;
OI Kohler, Frank/0000-0001-7150-6509; Strong, Ellen/0000-0001-7181-4114
FU Deutsche Forschungsgemeinschaft
FX This project was made possible through travel and research grants from
the Deutsche Forschungsgemeinschaft to FK, which are gratefully
acknowledged. Thanks for collecting permission and assistance in the
field to Ho Thanh Hai, Do Van Tu (Institute of Ecology and
Bio-Resources, Hanoi) and to Sabine Schutt (Berlin). We thank Larisa
Prozorova (Russian Academy of Sciences) for providing specimens of
'Parajuga' from Primorskiy Kray. We are grateful to Philippe Bouchet
(MNHN) for critically reading the manuscript and consulting on matters
of zoological nomenclature, to Chris Meyer (USNM) for informative
discussions on molecular clocks, and to Diarmaid O'Foighil (University
of Michigan) for providing constructive comments on molecular evolution
of freshwater cerithioideans. We also thank Marilyn Schotte (USNM) for
inking the anatomical drawings and Claudia Dames (ZMB) for SEM
examination of the radula.
NR 62
TC 13
Z9 14
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0300-3256
J9 ZOOL SCR
JI Zool. Scr.
PD SEP
PY 2009
VL 38
IS 5
BP 483
EP 502
DI 10.1111/j.1463-6409.2008.00385.x
PG 20
WC Evolutionary Biology; Zoology
SC Evolutionary Biology; Zoology
GA 483KD
UT WOS:000268962500003
ER
PT J
AU Santagata, S
Cohen, BL
AF Santagata, Scott
Cohen, Bernard L.
TI Phoronid phylogenetics (Brachiopoda; Phoronata): evidence from
morphological cladistics, small and large subunit rDNA sequences, and
mitochondrial cox1
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE actinotroch; Lophotrochozoa; pan-Brachiopoda; Phoronis; Phoronopsis;
Talpina
ID GEOLOGIC TIME-SCALE; 18S RIBOSOMAL DNA; REGIONAL SPECIFICATION; LARVAL
DEVELOPMENT; PALLIDA PHORONIDA; MOLECULAR EVIDENCE; GENE-SEQUENCES;
CLUSTAL-X; EVOLUTIONARY; PROTOSTOMES
AB A matrix of 24 morphodevelopmental characters and an alignment of small subunit (SSU) and large subunit (LSU) rDNA nuclear and cox1 mitochondrial gene sequences (similar to 4500 sites) were compiled from up to 12 phoronids including most named taxa, but probably constituting only a portion of worldwide diversity. Morphological data were analysed by weighted parsimony; sequence data by maximum and Bayesian likelihood, both with Phoronis ovalis as the local outgroup. Morphological and sequence-based phylogenies were similar, but not fully congruent. Phoronid rDNAs were almost free from mutational saturation, but cox1 showed strong saturation unless distant outgroups and P. ovalis were omitted, suggesting that many phoronid divergences are old (>= 100 Myr). rDNA divergence between named phoronid taxa is generally substantial, but Phoronopsis harmeri (from Vladivostock) and Phoronopsis viridis (from California) are genetically close enough to be conspecific. In another alignment, of 24 taxa, phoronid rDNAs were combined with data from brachiopods and distant (molluscan) outgroups. The relative ages of divergence between phoronids and their brachiopod sister-groups, of the split between the P. ovalis and non-ovalis lineages, and of other phoronid splits, were estimated from this alignment with a Bayesian lognormal uncorrelated molecular clock model. Although confidence limits (95% highest probability density) are wide, the results are compatible with an Early Cambrian split between phoronids and brachiopods and with the Upper Devonian latest age suggested for the P. ovalis/non-ovalis split by the putative phoronid ichnofossil, Talpina. Most other ingroup splits appear to be similar to 50-200 Myr old. Inclusion of phoronids with brachiopods in the crown clade pan-Brachiopoda suggests that a distinctive metamorphosis and absence of mineralization are ancestral phoronid apomorphies. Worldwide diversity and possible associations between character-states and life-history attributes deserve comprehensive further study. (C) 2009 The Linnean Society of London, Zoological Journal of the Linnean Society, 2009, 157, 34-50.
C1 [Cohen, Bernard L.] Univ Glasgow, FBLS Div Mol Genet, Glasgow G11 6NU, Lanark, Scotland.
[Santagata, Scott] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Cohen, BL (reprint author), Univ Glasgow, FBLS Div Mol Genet, Pontecorvo Bldg,56 Dumbarton Rd, Glasgow G11 6NU, Lanark, Scotland.
EM b.l.cohen@bio.gla.ac.uk
NR 84
TC 31
Z9 34
U1 0
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
EI 1096-3642
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD SEP
PY 2009
VL 157
IS 1
BP 34
EP 50
DI 10.1111/j.1096-3642.2009.00531.x
PG 17
WC Zoology
SC Zoology
GA 489BW
UT WOS:000269395500003
ER
PT J
AU Anker, A
Baeza, JA
De Grave, S
AF Anker, Arthur
Baeza, Juan Antonio
De Grave, Sammy
TI A New Species of Lysmata (Crustacea, Decapoda, Hippolytidae) from the
Pacific Coast of Panama, with Observations of Its Reproductive Biology
SO ZOOLOGICAL STUDIES
LA English
DT Article
DE Lysmata; Shrimp; New species; Eastern Pacific; Hermaphroditism
ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; MARINE SHRIMP; WESTERN
ATLANTIC; SEXUAL SYSTEM; CARIDEA; WURDEMANNI; REDESCRIPTION; INTERMEDIA
AB Arthur Anker, Juan Antonio Baeza, and Sammy De Grave (2009) A new species of Lysmata (Crustacea: Decapoda: Hippolytidae) from the Pacific coast of Panama, with observations of its reproductive biology. Zoological Studies 48(5): 682-692. Lysmata holthuisi sp. nov., a new peppermint shrimp, is described from Taboga I., on the Pacific coast of Panama. In addition to the type locality, L. holthuisi sp. nov. occurs in the vicinity of Panama City and around some islands relatively close to the mainland (Las Perlas and Coiba). The new species can be distinguished from other species of Lysmata by the rostrum bearing 6 (occasionally 5 or 7) dorsal and 2 (rarely 3) ventral teeth; the presence of setae between the dorsal rostral teeth; an acute well-developed pterygostomial tooth; a stylocerite overreaching the 1st antennular segment; the accessory branch of the lateral antennular flagellum consisting of 6 or 7 free segments; the marked segmentation of the merus of the 2nd pereiopod; the absence of a posteroventral tooth on the 4th pleuron; and by its diagnostic color pattern, characterized by red longitudinal stripes on the carapace and abdomen, and conspicuous bright yellow and red markings on or near the accessory branch of the lateral antennular flagellum. Among the eastern Pacific species, L. holthuisi sp. nov. appears to be most closely related to L. argentopunctata Wicksten and L, chica Wicksten. Anatomical observations, field population studies, and laboratory experiments indicate that L. holthuisi sp. nov. is a protandric simultaneous hermaphrodite, with an early male phase followed by a functional simultaneous hermaphroditic phase. http://zoolstud.sinica.edu.tw/Journals/48.5/682.pdf
C1 [De Grave, Sammy] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England.
[Baeza, Juan Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA.
[Anker, Arthur; Baeza, Juan Antonio] Inst Smithsonian Invest Trop, Balboa, Ancon, Panama.
RP De Grave, S (reprint author), Univ Oxford, Museum Nat Hist, Parks Rd, Oxford OX1 3PW, England.
EM arthuranker7@yahoo.com; baezaa@si.edu; sammydegrave@oum.ox.ac.uk
RI stud, zool/G-4030-2011;
OI De Grave, Sammy/0000-0002-2437-2445; Baeza, Juan
Antonio/0000-0002-2573-6773
FU Smithsonian Tropical Research Institute (STRI); Smithsonian Marine
Station at Fort Pierce, FL; USNM
FX P.C. Dworschak (Naturhistorisches Museum in Wien, Vienna, Austria) and
R. Lemaitre (USNM) are acknowledged for checking the type material of
Lysmata under their care. J.A. Vera Caripe (Universidad de Oriente, Boca
del Rio, Venezuela) prepared most of the initial drawings. AB
acknowledges the support of the Smithsonian Tropical Research Institute
(STRI) and the Smithsonian Marine Station at Fort Pierce, FL for
postdoctoral fellowships, as well as R. Colin and J. Christy (STRI) for
allowing the use of facilities and equipment in their laboratories. AA
is grateful to N. Knowlton (USNM) for financial support in the form of a
postdoctoral fellowship. This is contribution number 798 of the
Smithsonian Marine Station at Fort Pierce.
NR 21
TC 9
Z9 14
U1 0
U2 2
PU ACAD SINICA INST ZOOLOGY
PI TAIPEI
PA EDITORIAL OFFICE, TAIPEI 115, TAIWAN
SN 1021-5506
J9 ZOOL STUD
JI Zool. Stud.
PD SEP
PY 2009
VL 48
IS 5
BP 682
EP 692
PG 11
WC Zoology
SC Zoology
GA 502NE
UT WOS:000270466400012
ER
PT J
AU Klein, M
Hohensee, M
Nemiroski, A
Xiao, Y
Phillips, DF
Walsworth, RL
AF Klein, M.
Hohensee, M.
Nemiroski, A.
Xiao, Y.
Phillips, D. F.
Walsworth, R. L.
TI Slow light in narrow paraffin-coated vapor cells
SO APPLIED PHYSICS LETTERS
LA English
DT Article
DE alumina; atomic layer deposition; II-VI semiconductors; nanostructured
materials; optical materials; photonic band gap; refractive index;
self-assembly; titanium compounds; wide band gap semiconductors; zinc
compounds
ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; RELAXATION; CLOCK; MEDIA
AB We have self-assembled photonic crystal with a multistack structure using same size of spheres but from materials with different refractive indices. Al2O3, ZnO, and TiO2 are infiltrated into opal templates by atomic layer deposition. Stacking multiple inverse opal structures with different refractive index contrasts broadens the reflection bands dramatically. Numerical simulations with plane wave expansion method show good agreement with experimental results.
C1 [Klein, M.; Hohensee, M.; Xiao, Y.; Phillips, D. F.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Klein, M.; Hohensee, M.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Nemiroski, A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
RP Klein, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mklein@fas.harvard.edu
RI Nemiroski, Alex/A-9948-2011;
OI Hohensee, Michael/0000-0002-8106-4502
NR 26
TC 4
Z9 4
U1 0
U2 11
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD AUG 31
PY 2009
VL 95
IS 9
AR 091102
DI 10.1063/1.3207825
PG 3
WC Physics, Applied
SC Physics
GA 492AK
UT WOS:000269625800002
ER
PT J
AU Mengual, X
Ruiz, C
Rojo, S
Stahls, G
Thompson, FC
AF Mengual, Ximo
Ruiz, Carlos
Rojo, Santos
Stahls, Gunilla
Thompson, F. Christian
TI A conspectus of the flower fly genus Allograpta (Diptera: Syrphidae)
with description of a new subgenus and species
SO ZOOTAXA
LA English
DT Review
DE Costarica; identification key; Syrphinae; taxonomy
ID FLIES DIPTERA; MOLECULAR PHYLOGENY; SYSTEMATICS; CHARACTERS; HISTORY;
LARVAL
AB A new subgenus [Allograpta (Costarica Mengual & Thompson), type Allograpta zumbadoi Thompson], and one new species [ Allograpta ( Costarica) nishida Mengual & Thompson; type-locality: Costa Rica, type-depository: Instituto Nacional de Biodiversidad de Costa Rica] of flower flies ( Diptera: Syrphidae) are described from the Neotropical biotic region. A checklist of the world species of Allograpta including synonyms is provided, and a key to and diagnoses of the subgenera are also supplied. The phylogenetic relationships among Allograpta species, representing all hitherto detected morphological diversity of the genus, and related genera were studied under parsimony based on morphological characters.
C1 [Mengual, Ximo; Rojo, Santos] Univ Alicante, Inst Univ CIBIO, Dept Ciencias Ambientales & Recursos Nat, E-03080 Alicante, Spain.
[Ruiz, Carlos] Univ Valle, Dept Biol, Secc Entomol, Grp Invest Entomol, Ciudad Univ Melendez 25623, Colombia.
[Stahls, Gunilla] Univ Helsinki, Finnish Museum Nat Hist, Dept Entomol, FI-00014 Helsinki, Finland.
[Thompson, F. Christian] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA.
RP Mengual, X (reprint author), Univ Alicante, Inst Univ CIBIO, Dept Ciencias Ambientales & Recursos Nat, Apdo 99, E-03080 Alicante, Spain.
EM xmengual@ua.es; carlosruiz78@gmail.com; santos.rojo@ua.es;
gunilla.stahls@helsinki.fi; thompsonf@si.edu
OI Mengual, Ximo/0000-0002-6185-9404; Stahls, Gunilla/0000-0003-0505-0691
FU Schlinger Foundation; USDA
FX We thank Wayne N. Mathis, Department of Entomology, Smithsonian
Institution, Washington, and Natalia Vanderberg, Allen Norrbom, and Alma
Solis, Systematic Entomology Laboratory, USDA, Washington, for their
critical reviews of the manuscript. The original version of the
manuscript was produced and submitted while the senior author ( in age,
that is) was an employee of the US Department of Agriculture. Major
revisions were made after his forced retirement and while he was an
adjunct and emeritus scientist with the Smithsonian Institution, where
Ximo Mengual is now currently a post-doctoral research fellow supported
by the Schlinger Foundation. So, we acknowledge their continued support
and acknowledge USDA decision to no longer support research on flower
flies.
NR 136
TC 10
Z9 11
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 AUG 31
PY 2009
IS 2214
BP 1
EP 28
PG 28
WC Zoology
SC Zoology
GA 490GU
UT WOS:000269488900001
ER
PT J
AU Nilsson, T
Davis, JL
Hill, EM
AF Nilsson, T.
Davis, J. L.
Hill, E. M.
TI Using ground-based GPS to characterize atmospheric turbulence
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WATER-VAPOR
AB A new method for measuring and studying atmospheric turbulence is presented. The method uses data from a local network of GPS receivers. The GPS data are processed in a way that assures that the estimated zenith total delays (ZTD) contain the effects of atmospheric turbulence present in the GPS observations. The turbulence is characterized using the spatial structure function for the atmospheric zenith total delay. The structure function is modeled by an expression with unknown parameters which contains information about the turbulence. The unknown parameters are solved by a fit to the observed ZTD variations. We apply the method to GPS data from the Yucca Mountain network, Nevada, USA. The results show that the magnitude of the turbulent variations in that region have a strong seasonal dependence, with much larger variations in summer compared to winter. Citation: Nilsson, T., J. L. Davis, and E. M. Hill (2009), Using ground-based GPS to characterize atmospheric turbulence, Geophys. Res. Lett., 36, L16807, doi: 10.1029/2009GL040090.
C1 [Nilsson, T.] Chalmers, Dept Radio & Space Sci, SE-41296 Gothenburg, Sweden.
[Davis, J. L.; Hill, E. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nilsson, T.] Vienna Univ Technol, Inst Geodesy & Geophys, A-1040 Vienna, Austria.
RP Nilsson, T (reprint author), Chalmers, Dept Radio & Space Sci, SE-41296 Gothenburg, Sweden.
EM tobias.nilsson@chalmers.se; jdavis@cfa.harvard.edu;
ehill@cfa.harvard.edu
RI Hill, Emma/B-7037-2011; Nilsson, Tobias/D-3764-2012; Davis,
James/D-8766-2013
OI Hill, Emma/0000-0003-0231-5818; Nilsson, Tobias/0000-0003-4103-9078;
Davis, James/0000-0003-3057-477X
FU Swedish National Space Board
FX The research on atmospheric turbulence by Tobias Nilsson was supported
by the Swedish National Space Board.
NR 14
TC 9
Z9 9
U1 0
U2 2
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 AUG 29
PY 2009
VL 36
AR L16807
DI 10.1029/2009GL040090
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 488KS
UT WOS:000269349100006
ER
PT J
AU Laurance, W
AF Laurance, William
TI Roads to ruin
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Laurance, William] Smithsonian Trop Res Inst Panama, Panama City, Panama.
NR 0
TC 2
Z9 2
U1 1
U2 4
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD AUG 29
PY 2009
VL 203
IS 2723
BP 24
EP 25
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 491HT
UT WOS:000269570200017
ER
PT J
AU Carleton, MD
Emmons, LH
Musser, GG
AF Carleton, Michael D.
Emmons, Louise H.
Musser, Guy G.
TI A New Species of the Rodent Genus Oecomys (Cricetidae: Sigmodontinae:
Oryzomyini) from Eastern Bolivia, with Emended Definitions of O.
concolor (Wagner) and O. mamorae (Thomas)
SO AMERICAN MUSEUM NOVITATES
LA English
DT Article
ID MAMMALS; DIVERSIFICATION; EVOLUTIONARY; COLOMBIA; PATTERNS; MUROIDEA;
MURIDAE; HISTORY
AB We describe a new species of Oecomys, O. sydandersoni (Cricetidae: Sigmodontinae), from the Parque Nacional Noel Kempff Mercado in eastern Bolivia. One of its diagnostic traits, a derived carotid circulatory plan, provides morphological evidence for its close relationship to O. concolor and O. mamorae among the 15 species of Oecomys currently recognized. Notwithstanding this shared trait, other morphological contrasts and morphometric analyses demonstrate the sharp differentiation of the eastern Bolivian form from both of those species. Oecomys sydandersoni, n. sp., is arboreal and was encountered above ground on limbs and woody vines only in densely wooded hummocks scattered through grassland, in contrast to adjacent closed tropical deciduous forest where three other species of Oecomys (O. bicolor, O. roberti, O. trinitatis) were obtained. The new species represents the fourth sigmodontine rodent to be named from this restricted region within eastern Bolivia since 1999. Its documentation served as a platform to summarize the nomenclatural history, morphological recognition, and geographic distribution of O. concolor (Wagner, 1845) and O. mamorae (Thomas, 1906) based on fresh examination of all type material and museum specimens.
C1 [Carleton, Michael D.; Emmons, Louise H.; Musser, Guy G.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, Washington, DC 20560 USA.
[Carleton, Michael D.; Emmons, Louise H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Carleton, MD (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammal, Washington, DC 20560 USA.
EM carletonm@si.edu; emmonsl@si.edu; holdenmusser@charter.net
NR 64
TC 11
Z9 12
U1 0
U2 5
PU AMER MUSEUM NATURAL HISTORY
PI NEW YORK
PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT
79TH ST, NEW YORK, NY 10024-5192 USA
SN 0003-0082
EI 1937-352X
J9 AM MUS NOVIT
JI Am. Mus. Novit.
PD AUG 28
PY 2009
IS 3661
BP 1
EP 32
PG 32
WC Biodiversity Conservation; Zoology
SC Biodiversity & Conservation; Zoology
GA 489WE
UT WOS:000269455200001
ER
PT J
AU Chesser, RT
Claramunt, S
Derryberry, E
Brumfield, RT
AF Chesser, R. Terry
Claramunt, Santiago
Derryberry, Elizabeth
Brumfield, Robb T.
TI Geocerthia, a new genus of terrestrial ovenbird (Aves: Passeriformes:
Furnariidae)
SO ZOOTAXA
LA English
DT Letter
ID UPUCERTHIA; PHYLOGENY; EVOLUTION
C1 [Chesser, R. Terry] USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
[Claramunt, Santiago; Derryberry, Elizabeth; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Claramunt, Santiago; Derryberry, Elizabeth; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
RP Chesser, RT (reprint author), USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, POB 37012, Washington, DC 20013 USA.
RI Derryberry, Elizabeth/C-2396-2011;
OI Brumfield, Robb/0000-0003-2307-0688
NR 11
TC 3
Z9 5
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 AUG 28
PY 2009
IS 2213
BP 64
EP 68
PG 5
WC Zoology
SC Zoology
GA 489SK
UT WOS:000269442500004
ER
PT J
AU Brizzi, G
Arnone, E
Carlotti, M
Dinelli, BM
Flaud, JM
Papandrea, E
Perrin, A
Ridolfi, M
AF Brizzi, G.
Arnone, E.
Carlotti, M.
Dinelli, B. M.
Flaud, J. -M.
Papandrea, E.
Perrin, A.
Ridolfi, M.
TI Retrieval of atmospheric (HNO3)-N-15/(HNO3)-N-14 isotope ratio profile
from MIPAS/ENVISAT limb-scanning measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID EMISSION-SPECTRA; NITRIC-ACID; SATELLITE MEASUREMENTS; AIRCRAFT
MEASUREMENTS; ATMOS EXPERIMENT; HNO3 PROFILES; MIPAS; STRATOSPHERE;
FRACTIONATION; CLONO2
AB We report the first measurement of the isotopic partitioning between stratospheric (HNO3)-N-14 and (HNO3)-N-15. The vertical distribution of the isotope ratio of the two isotopologues of nitric acid was derived using the nu(5) band Q branch of (HNO3)-N-15 that was recently identified in measurements from the MIPAS experiment using newly generated spectral line parameters for the minor isotopologue. Because of the very low intensity of the spectral features adopted for the retrieval, we established an "ad hoc" inversion procedure based on a regularized linear Kalman filter approach. This procedure permits the retrieval of the deviations from the natural (HNO3)-N-15/(HNO3)-N-14 isotope ratio profile, averaged over different latitude bands and time intervals, in the altitude range from 18 to 42 km. The resulting profiles show an overall substantial depletion with height of (HNO3)-N-15, with respect to the natural partitioning, and no significant latitude and time dependence. The developed retrieval procedure can be readily extended to other atmospheric trace gas isotope ratios.
C1 [Brizzi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Arnone, E.; Carlotti, M.; Papandrea, E.; Ridolfi, M.] Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy.
[Dinelli, B. M.] CNR, Ist Sci Atmosfera & Clima, I-40129 Bologna, Italy.
[Flaud, J. -M.; Perrin, A.] Univ Paris 12, Univ Paris 07, Lab Interuniv Syst Atmospher, CNRS, F-94010 Creteil, France.
RP Brizzi, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-50, Cambridge, MA 02138 USA.
EM gbrizzi@cfa.harvard.edu; arnone@fci.unibo.it; carlotti@fci.unibo.it;
bm.dinelli@isac.cnr.it; flaud@lisa.univ-paris12.fr;
enzo@safire.fci.unibo.it; agnes.perrin@lisa.univ-paris12.fr;
ridolfi@fci.unibo.it
RI Dinelli, Bianca Maria/C-1212-2015;
OI Papandrea, Enzo/0000-0001-6698-0011
FU NASA [NNG05GO08G]; European Community's Human Potential Programme Marie
Curie [MERG-CT-2007-209157]
FX The authors are grateful to Simone Ceccherini for fruitful discussions
regarding the retrieval approach developed as part of this work. G.
Brizzi gratefully acknowledges Kelly Chance for the valuable opportunity
of working at CfA and funding through the NASA grant NNG05GO08G. E.
Arnone acknowledges funding through the European Community's Human
Potential Programme Marie Curie under contract MERG-CT-2007-209157.
NR 50
TC 5
Z9 5
U1 0
U2 1
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 AUG 25
PY 2009
VL 114
AR D16301
DI 10.1029/2008JD011504
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 488KY
UT WOS:000269349800002
ER
PT J
AU Fukui, Y
Furukawa, N
Dame, TM
Dawson, JR
Yamamoto, H
Rowell, GP
Aharonian, F
Hofmann, W
Wilhelmi, ED
Minamidani, T
Kawamura, A
Mizuno, N
Onishi, T
Mizuno, A
Nagataki, S
AF Fukui, Yasuo
Furukawa, Naoko
Dame, Thomas M.
Dawson, Joanne R.
Yamamoto, Hiroaki
Rowell, Gavin P.
Aharonian, Felix
Hofmann, Werner
Wilhelmi, Emma de Ona
Minamidani, Tetsuhiro
Kawamura, Akiko
Mizuno, Norikazu
Onishi, Toshikazu
Mizuno, Akira
Nagataki, Shigehiro
TI A Peculiar Jet and Arc of Molecular Gas toward the Rich and Young
Stellar Cluster Westerlund 2 and a TeV Gamma Ray Source
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE acceleration of particles; ISM: molecules; stars: individual (Westerlund
2); stars: supernovae: general
ID SUPERNOVA EXPLOSIONS; CLOUD FORMATION; GALACTIC PLANE; EMISSION;
TELESCOPE; PULSARS; CORE
AB We have discovered remarkable jet- and arc-like molecular features toward the rich and young stellar cluster Westerlund 2. The jet has a length of similar to 100 pc and a width of similar to 10 pc, while the are shows a crescent shape with a radius of similar to 30 pc. These molecular features each have masses of similar to 10(4) M-circle dot, and show spatial correlations with the surrounding lower density H I gas. The jet also shows an intriguing positional alignment with the core of the TeV gamma-ray source HESS J1023-575 and with the MeV/GeV gamma-ray source recently reported by the Fermi collaboration. We argue that the jet and arc are caused by an energetic event in Westerlund 2, presumably due to an anisotropic supernova explosion of one of the most massive member stars. While the origin of the TeV and GeV gamma-ray sources is uncertain, one may speculate that they are related to the same event via relativistic particle acceleration by strong shock waves produced at the explosion or by remnant objects, such as a pulsar wind nebula or a microquasar.
C1 [Fukui, Yasuo; Furukawa, Naoko; Dawson, Joanne R.; Yamamoto, Hiroaki; Kawamura, Akiko; Mizuno, Norikazu; Onishi, Toshikazu] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Dame, Thomas M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dawson, Joanne R.] Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Rowell, Gavin P.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Aharonian, Felix] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Aharonian, Felix; Hofmann, Werner; Wilhelmi, Emma de Ona] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Minamidani, Tetsuhiro] Hokkaido Univ, Fac Sci, Dept Phys, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Mizuno, Norikazu] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Onishi, Toshikazu] Osaka Prefecture Univ, Dept Phys Sci, Naka Ku, Sakai, Osaka 5998531, Japan.
[Mizuno, Akira] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Nagataki, Shigehiro] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
RP Fukui, Y (reprint author), Nagoya Univ, Dept Astrophys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
EM fukui@a.phys.nagoya-u.ac.jp
OI Minamidani, Tetsuhiro/0000-0001-9778-6692; de Ona Wilhelmi,
Emma/0000-0002-5401-0744
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT)
[15071101, 15071203]; Japan Society for the Promotion of Science
[20244014, 21253003]; MEXT [17004]; Mitsubishi Foundation
FX The original NANTEN telescope was operated based on a mutual agreement
between Nagoya University and the Carnegie Institution of Washington.
This work is financially supported in part by a Grants-in-Aid for
Scientific Research (KAKENHI) from the Ministry of Education, Culture,
Sports, Science and Technology (MEXT) (Nos. 15071101 and 15071203) and
from Japan Society for the Promotion of Science (Nos. 20244014 and
21253003). This work is also financially supported in part by
core-to-core program of a Grant-in-Aid for Scientific Research from the
MEXT (No. 17004), the Mitsubishi Foundation and by the donation from
individuals and private companies.
NR 26
TC 13
Z9 13
U1 0
U2 3
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 AUG 25
PY 2009
VL 61
IS 4
BP L23
EP L27
DI 10.1093/pasj/61.4.L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 513ZX
UT WOS:000271364000003
ER
PT J
AU Young, AJ
Monfort, SL
AF Young, Andrew J.
Monfort, Steven L.
TI Stress and the costs of extra-territorial movement in a social carnivore
SO BIOLOGY LETTERS
LA English
DT Article
DE cooperative breeding; extra group; allostatic load
ID REPRODUCTION; DISPERSAL; MEERKATS; HORMONES
AB Costs associated with extra-territorial movement are believed to have favoured the evolution of delayed dispersal and sociality across a range of social vertebrates, but remain surprisingly poorly understood. Here we reveal a novel mechanism that may contribute substantially to the costs of extra-territorial movement: physiological stress. We show that subordinate male meerkats, Suricata suricatta, exhibit markedly elevated faecal glucocorticoid metabolite levels (a non-invasive measure of hypothalamic pituitary -adrenal axis activity) while conducting extra-territorial prospecting forays. While brief increases in glucocorticoid levels are unlikely to be costly, chronic elevations, arising from prolonged and/or frequent forays, are expected to compromise fitness through their diverse negative effects on health. Our findings strongly suggest that prolonged extra-territorial movements do result in chronic stress, as the high glucocorticoid levels of prospectors do not diminish on longer forays and are no lower among males with greater prospecting experience. A generalized 'stress' of extra-territorial movement may therefore have strengthened selection for delayed dispersal and sociality in this and other species, and favoured the conduct of brief forays over extended periods of floating. Our findings have implications too for understanding the rank-related distribution of physiological stress in animal societies, as extra-territorial movements are often conducted solely by subordinates.
C1 [Young, Andrew J.] Univ Exeter, Ctr Ecol & Conservat, Tremough TR10 9EZ, Cornwall, England.
[Young, Andrew J.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Monfort, Steven L.] Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA.
RP Young, AJ (reprint author), Univ Exeter, Ctr Ecol & Conservat, Cornwall Campus, Tremough TR10 9EZ, Cornwall, England.
EM a.j.young@exeter.ac.uk
FU Natural Environment Research Council, Magdalene College, Cambridge;
Smithsonian Institution
FX We thank the Mammal Research Institute, University of Pretoria and our
volunteers their for valuable assistance, Tim Clutton-Brock for access
to the study population and research supervision, and the Natural
Environment Research Council, Magdalene College, Cambridge and the
Smithsonian Institution for funding.
NR 11
TC 29
Z9 29
U1 3
U2 26
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1744-9561
J9 BIOL LETTERS
JI Biol. Lett.
PD AUG 23
PY 2009
VL 5
IS 4
BP 439
EP 441
DI 10.1098/rsbl.2009.0032
PG 3
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 469FQ
UT WOS:000267881700001
PM 19324630
ER
PT J
AU Yanoviak, SP
Kaspari, M
Dudley, R
AF Yanoviak, Stephen P.
Kaspari, Michael
Dudley, Robert
TI Gliding hexapods and the origins of insect aerial behaviour
SO BIOLOGY LETTERS
LA English
DT Article
DE aerial gliding; Archaeognatha; evolution; flight; tropics
ID EVOLUTIONARY PATHWAY; FLIGHT; DESCENT
AB Directed aerial descent (i.e. gliding and manoeuvring) may be an important stage in the evolution of winged flight. Although hypothesized to occur in ancestrally wingless insects, such behaviour is unexplored in extant basal hexapods, but has recently been described in arboreal ants. Here we show that tropical arboreal bristletails (Archaeognatha) direct their horizontal trajectories to tree trunks in approximately 90 per cent of falls. Experimental manipulation of the median caudal filament significantly reduced both success rate (per cent of individuals landing on a tree trunk) and performance (glide index) versus controls. The existence of aerial control in the ancestrally wingless bristletails, and its habitat association with an arboreal lifestyle, are consistent with the hypothesis of a terrestrial origin for winged flight in insects.
C1 [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
[Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA.
[Kaspari, Michael; Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama.
[Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
RP Yanoviak, SP (reprint author), Univ Arkansas, Dept Biol, 2801 S Univ Ave, Little Rock, AR 72204 USA.
EM spyanoviak@ualr.edu
OI Kaspari, Michael/0000-0002-9717-5768
FU Smithsonian Monitoring and Assessing Biodiversity Program; National
Zoological Park; National Science Foundation [IOS-0837866]; National
Geographic Society [CRE 7896-05]
FX We thank J. Kingsolver, M. Knornschild, S. Price, S. Revzen, R. Verble
and the UC Berkeley biomechanics group for their comments. O. Acevedo,
A. Alonso, P. Bucur, F. Dallmeier, A. Henderson, A. Honorez, P. Jensen,
M. Lee, S. Madigosky, T. Pacheco and O. S. G. Pauwels provided
logistical support. A. Mikheyev, G. Moussavou and E. Tobi assisted in
the field, and R. Molero Baltanas (Universidad de Cordoba) identified
the bristletails. We also thank the Amazon Conservatory for Tropical
Studies, Amazon Explorama Lodges, Shell Gabon, and the private
landowners who facilitated access to field sites. This research was
supported in part by the Smithsonian Monitoring and Assessing
Biodiversity Program, the National Zoological Park, the National Science
Foundation (IOS-0837866) and the National Geographic Society (CRE
7896-05).
NR 16
TC 23
Z9 24
U1 0
U2 26
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1744-9561
J9 BIOL LETTERS
JI Biol. Lett.
PD AUG 23
PY 2009
VL 5
IS 4
BP 510
EP 512
DI 10.1098/rsbl.2009.0029
PG 3
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 469FQ
UT WOS:000267881700021
PM 19324632
ER
PT J
AU Wyithe, JSB
Loeb, A
AF Wyithe, J. Stuart B.
Loeb, Abraham
TI The 21-cm power spectrum after reionization
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; intergalactic medium; diffuse radiation
ID DAMPED LY-ALPHA; BARYONIC ACOUSTIC-OSCILLATIONS; HALO OCCUPATION
DISTRIBUTION; REDSHIFT-SPACE DISTORTIONS; LUMINOUS RED GALAXIES;
ABSORPTION SYSTEMS; STAR-FORMATION; INTERGALACTIC MEDIUM; DARK-MATTER;
FLUCTUATIONS
AB We discuss the 21-cm power spectrum (PS) following the completion of reionization. In contrast to the reionization era, this PS is proportional to the PS of mass density fluctuations, with only a small modulation due to fluctuations in the ionization field on scales larger than the mean-free-path of ionizing photons. We derive the form of this modulation, and demonstrate that its effect on the 21-cm PS will be smaller than 1 per cent for physically plausible models of damped Ly alpha systems. In contrast to the 21-cm PS observed prior to reionization, in which H ii regions dominate the ionization structure, the simplicity of the 21-cm PS after reionization will enhance its utility as a cosmological probe by removing the need to separate the PS into physical and astrophysical components. As a demonstration, we consider the Alcock-Paczynski test and show that the next generation of low-frequency arrays could measure the angular distortion of the PS at the per cent level for z similar to 3-5.
C1 [Wyithe, J. Stuart B.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia.
[Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wyithe, JSB (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia.
EM swyithe@unimelb.edu.au; loeb@cfa.harvard.edu
OI Wyithe, Stuart/0000-0001-7956-9758
FU Australian Research Council (JSBW); NASA [NNX08AL43G, LA]; FQXi; Harvard
University
FX The research was supported by the Australian Research Council (JSBW), by
NASA grants NNX08AL43G and LA, by FQXi, and by Harvard University funds
(AL).
NR 45
TC 19
Z9 19
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 21
PY 2009
VL 397
IS 4
BP 1926
EP 1934
DI 10.1111/j.1365-2966.2009.15019.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 483IU
UT WOS:000268958400018
ER
PT J
AU Tang, YP
Gu, QS
Huang, JS
Wang, YP
AF Tang, Yuping
Gu, Q. -S.
Huang, J. -S.
Wang, Y. -P.
TI Infrared-red cores in nearby elliptical galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: elliptical and lenticular; cD; galaxies:
nuclei; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; DWARF SEYFERT NUCLEI;
SPECTRAL ENERGY-DISTRIBUTIONS; ARRAY CAMERA IRAC; SPATIAL-DISTRIBUTION;
SPITZER OBSERVATIONS; INTERSTELLAR MATTER; SURFACE BRIGHTNESS; RADIO
LUMINOSITY
AB We present the Spitzer Space Telescope Infrared Array Camera observations for a sample of local elliptical galaxies to study later stages of active galactic nucleus (AGN) activity. A sample of 36 elliptical galaxies is selected from the Palomar spectroscopic survey. We detect nuclear non-stellar infrared emission in nine of them. There is unambiguous evidence of circumnuclear dust in these nine galaxies in their optical images. We also find a remarkable correlation between the infrared excess emission and the nuclear radio/X-ray emission, suggesting that infrared excess emission is tightly related to nuclear activity. The possible origin of infrared excess emission from hot dust heated by the central AGN is supported by the spectral indices of the infrared excess emission.
C1 [Tang, Yuping; Gu, Q. -S.; Wang, Y. -P.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tang, YP (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
EM tangyping@gmail.com; qsgu@nju.edu.cn
FU Program for New Century Excellent Talents in University (NCET); national
Natural Science Foundation of China [10878010, 10633040]; National Basic
Research Program (973 Program) [2007CB815405]; Jet Propulsion
Laboratory, California Institute of Technology; National Aeronautics and
Space Administration; NASA [1407]
FX We are very grateful to Tom Jarrett and Feng Yuan for their valuable
advice. We are also thankful to Tao Wang and Song Huang for helpful
suggestions. This work was supported by the Program for New Century
Excellent Talents in University (NCET), the national Natural Science
Foundation of China under grants 10878010 and 10633040, and the National
Basic Research Program (973 Program No. 2007CB815405). This research has
made use of NASA's Astrophysics Data System Bibliographic Services and
the NASA/IPAC Extragalactic Data base (NED), which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
work is based on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under NASA contract 1407.
NR 89
TC 10
Z9 10
U1 0
U2 2
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 21
PY 2009
VL 397
IS 4
BP 1966
EP 1975
DI 10.1111/j.1365-2966.2009.15038.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 483IU
UT WOS:000268958400022
ER
PT J
AU Rick, TC
Erlandson, JM
AF Rick, Torben C.
Erlandson, Jon M.
TI Coastal Exploitation
SO SCIENCE
LA English
DT Editorial Material
ID SOUTH-AFRICA; ECOSYSTEMS; MIDDLE
C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA.
[Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA.
[Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA.
EM rickt@si.edu; jerland@uoregon.edu
OI Erlandson, Jon/0000-0002-4705-4319
NR 14
TC 33
Z9 35
U1 0
U2 23
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 21
PY 2009
VL 325
IS 5943
BP 952
EP 953
DI 10.1126/science.1178539
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 487AN
UT WOS:000269242800030
PM 19696338
ER
PT J
AU Kallman, TR
Bautista, MA
Goriely, S
Mendoza, C
Miller, JM
Palmeri, P
Quinet, P
Raymond, J
AF Kallman, T. R.
Bautista, M. A.
Goriely, Stephane
Mendoza, Claudio
Miller, Jon M.
Palmeri, Patrick
Quinet, Pascal
Raymond, John
TI SPECTRUM SYNTHESIS MODELING OF THE X-RAY SPECTRUM OF GRO J1655-40 TAKEN
DURING THE 2005 OUTBURST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: spectroscopic; black hole physics;
relativity
ID ACCRETION DISKS; BLACK-HOLE; IONIZATION EQUILIBRIUM; ABSORPTION-LINE;
MASS; WINDS; PHOTOIONIZATION; SPECTROSCOPY; QUIESCENCE; EVOLUTION
AB The spectrum from the black hole X-ray transient GRO J1655-40 obtained using the Chandra High Energy Transmission Grating in 2005 is notable as a laboratory for the study of warm absorbers, and for the presence of many lines from odd-Z elements between Na and Co ( and Ti and Cr) not previously observed in X-rays. We present synthetic spectral models which can be used to constrain these element abundances and other parameters describing the outflow from the warm absorber in this object. We present results of fitting to the spectrum using various tools and techniques, including automated line fitting, phenomenological models, and photoionization modeling. We show that the behavior of the curves of growth of lines from H-like and Li-like ions indicate that the lines are either saturated or affected by filling-in from scattered or a partially covered continuum source. We confirm the conclusion of previous work by Miller et al., which shows that the ionization conditions are not consistent with wind driving due to thermal expansion. The spectrum provides the opportunity to measure abundances for several elements not typically observable in the X-ray band. These show a pattern of enhancement for iron peak elements, and solar or subsolar values for elements lighter than calcium. Models show that this is consistent with enrichment by a core-collapse supernova. We discuss the implications of these values for the evolutionary history of this system.
C1 [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bautista, M. A.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA.
[Goriely, Stephane] Univ Libre Bruxelles, Inst Astron & Astrophys, B-1050 Brussels, Belgium.
[Mendoza, Claudio] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Palmeri, Patrick; Quinet, Pascal] Univ Mons, B-7000 Mons, Belgium.
[Raymond, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kallman, TR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU Chandra theory program
FX This work was funded in part by a grant from the Chandra theory program.
We thank the referee, Frits Paerels, for many constructive comments.
NR 42
TC 39
Z9 39
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 865
EP 884
DI 10.1088/0004-637X/701/2/865
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500002
ER
PT J
AU Shapiro, KL
Genzel, R
Quataert, E
Schreiber, NMF
Davies, R
Tacconi, L
Armus, L
Bouche, N
Buschkamp, P
Cimatti, A
Cresci, G
Daddi, E
Eisenhauer, F
Erb, DK
Genel, S
Hicks, EKS
Lilly, SJ
Lutz, D
Renzini, A
Shapley, A
Steidel, CC
Sternberg, A
AF Shapiro, Kristen L.
Genzel, Reinhard
Quataert, Eliot
Schreiber, Natascha M. Foerster
Davies, Richard
Tacconi, Linda
Armus, Lee
Bouche, Nicolas
Buschkamp, Peter
Cimatti, Andrea
Cresci, Giovanni
Daddi, Emanuele
Eisenhauer, Frank
Erb, Dawn K.
Genel, Shy
Hicks, Erin K. S.
Lilly, Simon J.
Lutz, Dieter
Renzini, Alvio
Shapley, Alice
Steidel, Charles C.
Sternberg, Amiel
TI THE SINS SURVEY: BROAD EMISSION LINES IN HIGH-REDSHIFT STAR-FORMING
GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift
ID ACTIVE GALACTIC NUCLEI; INTEGRAL FIELD SPECTROSCOPY; BLACK-HOLE MASS;
LYMAN-BREAK GALAXIES; OPTICAL LUMINOSITY DENSITY; FAR-INFRARED GALAXIES;
TO 2 GALAXIES; SUBMILLIMETER GALAXIES; SUPERNOVA-REMNANTS; RADIATION
PRESSURE
AB High signal-to-noise, representative spectra of star-forming galaxies at z similar to 2, obtained via stacking, reveal a high-velocity component underneath the narrow H alpha and [ N II] emission lines. When modeled as a single Gaussian, this broad component has FWHM greater than or similar to 1500 km s(-1); when modeled as broad wings on the H alpha and [ N II] features, it has FWHM greater than or similar to 500 km s(-1). This feature is preferentially found in the more massive and more rapidly star-forming systems, which also tend to be older and larger galaxies. We interpret this emission as evidence of either powerful starburst-driven galactic winds or active supermassive black holes ( SMBHs). If galactic winds are responsible for the broad emission, the observed luminosity and velocity of this gas imply mass outflow rates comparable to the star formation rate. On the other hand, if the broad-line regions of active black holes account for the broad feature, the corresponding black holes masses are estimated to be an order of magnitude lower than those predicted by local scaling relations, suggesting a delayed assembly of SMBHs with respect to their host bulges.
C1 [Shapiro, Kristen L.; Quataert, Eliot] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Genzel, Reinhard] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Genzel, Reinhard; Schreiber, Natascha M. Foerster; Davies, Richard; Tacconi, Linda; Bouche, Nicolas; Buschkamp, Peter; Cresci, Giovanni; Eisenhauer, Frank; Genel, Shy; Hicks, Erin K. S.; Lutz, Dieter] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Armus, Lee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Cimatti, Andrea] Osservatorio Astron Bologna, Ist Nazl Astrofis, I-40129 Bologna, Italy.
[Daddi, Emanuele] Dapnia CEA, Serv Astrophys, Saclay, France.
[Erb, Dawn K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lilly, Simon J.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Shapley, Alice] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Renzini, Alvio] Osserv Astron Padova, I-35122 Padua, Italy.
[Sternberg, Amiel] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
RP Shapiro, KL (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RI Daddi, Emanuele/D-1649-2012;
OI Daddi, Emanuele/0000-0002-3331-9590; Genel, Shy/0000-0002-3185-1540;
Cresci, Giovanni/0000-0002-5281-1417
NR 85
TC 49
Z9 49
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 955
EP 963
DI 10.1088/0004-637X/701/2/955
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500007
ER
PT J
AU Franco-Hernandez, R
Moran, JM
Rodriguez, LF
Garay, G
AF Franco-Hernandez, Ramiro
Moran, James M.
Rodriguez, Luis F.
Garay, Guido
TI THE ROTATING MOLECULAR STRUCTURES AND THE IONIZED OUTFLOW ASSOCIATED
WITH IRAS 16547-4247
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: individual (IRAS 16547-4247)
ID MASSIVE STAR-FORMATION; COLLIMATED JET SOURCE; H2O MASERS; SULFUR
CHEMISTRY; PROPER MOTIONS; HOT CORES; IRAS-16547-4247; REGIONS;
PROTOSTAR; ENVELOPES
AB We present Very Large Array 1.3 cm radio continuum and water maser observations as well as Submillimeter Array SO(2) ( 226.300 GHz) and 1.3 mm dust continuum observations toward the massive star formation region IRAS 16547-4247. We find evidence of multiple sources in the central part of the region. There is evidence of a rotating structure associated with the most massive of these sources, traced at small scales (similar to 50 AU) by the water masers. At large scales (similar to 1000 AU), we find a velocity gradient in the SO2 molecular emission with a barely resolved structure that can be modeled as a rotating ring or two separate objects. The velocity gradients of the masers and of the molecular emission have the same sense and may trace the same structure at different size scales. The position angles of the structures associated with the velocity gradients are roughly perpendicular to the outflow axis observed in radio continuum and several molecular tracers. We estimate the mass of the most massive central source to be around 30 solar masses from the velocity gradient in the water maser emission. The main source of error in this estimate is the radius of the rotating structure. We also find water masers that are associated with the large-scale molecular outflow of the system, as well as water masers that are associated with other sources in the region. Our results suggest that the formation of this source, one of the most luminous protostars or protostellar clusters known, is taking place with the presence of ionized jets and disk-like structures.
C1 [Franco-Hernandez, Ramiro; Moran, James M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Franco-Hernandez, Ramiro; Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
[Garay, Guido] Univ Chile, Dept Astron, Santiago, Chile.
RP Franco-Hernandez, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfranco@cfa.harvard.edu
RI Garay, Guido/H-8840-2013;
OI Garay, Guido/0000-0003-1649-7958; Moran, James/0000-0002-3882-4414
FU SAO; CONACyT, Mexico; DGAPA, UNAM; CONICYT [15010003, PFB-06]
FX We thank an anonymous referee for comments that improved two sections of
the paper and for the suggestion of discussing the possibility of
significant accretion luminosity. R. F. H. is grateful for support from
an SAO predoctoral fellowship. L. F. R. acknowledges the support of
CONACyT, Mexico and DGAPA, UNAM. G. G. acknowledges support from CONICYT
projects FONDAP no. 15010003 and BASAL PFB-06.
NR 38
TC 20
Z9 20
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 974
EP 983
DI 10.1088/0004-637X/701/2/974
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500009
ER
PT J
AU Gou, LJ
McClintock, JE
Liu, JF
Narayan, R
Steiner, JF
Remillard, RA
Orosz, JA
Davis, SW
Ebisawa, K
Schlegel, EM
AF Gou, Lijun
McClintock, Jeffrey E.
Liu, Jifeng
Narayan, Ramesh
Steiner, James F.
Remillard, Ronald A.
Orosz, Jerome A.
Davis, Shane W.
Ebisawa, Ken
Schlegel, Eric M.
TI A DETERMINATION OF THE SPIN OF THE BLACK HOLE PRIMARY IN LMC X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; black hole physics; galaxies: individual (LMC);
X-rays: binaries
ID LARGE-MAGELLANIC-CLOUD; ANGULAR-MOMENTUM TRANSPORT; ACCRETION DISK
MODELS; RAY-TIMING-EXPLORER; XMM-NEWTON/EPIC-PN; X-RAY; HIGH-STATE; M33
X-7; BINARY; CANDIDATE
AB The first extragalactic X-ray binary, LMC X-1, was discovered in 1969. In the 1980s, its compact primary was established as the fourth dynamical black hole candidate. Recently, we published accurate values for the mass of the black hole and the orbital inclination angle of the binary system. Building on these results, we have analyzed 53 X-ray spectra obtained by RXTE and, using a selected sample of 18 of these spectra, we have determined the dimensionless spin parameter of the black hole to be a(*) = 0.92(-0.07)(+0.05). This result takes into account all sources of observational and model-parameter uncertainties. The standard deviation around the mean value of a(*) for these 18 X-ray spectra, which were obtained over a span of several years, is only Delta a(*) = 0.02. When we consider our complete sample of 53 RXTE spectra, we find a somewhat higher value of the spin parameter and a larger standard deviation. Finally, we show that our results based on RXTE data are confirmed by our analyses of selected X-ray spectra obtained by the XMM-Newton, BeppoSAX, and Ginga missions.
C1 [Gou, Lijun; McClintock, Jeffrey E.; Liu, Jifeng; Narayan, Ramesh; Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Davis, Shane W.] Inst Adv Study, Princeton, NJ 08540 USA.
[Ebisawa, Ken] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Schlegel, Eric M.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA.
RP Gou, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA [NNX08AJ55G, NNX08AH32G, HST-GO-11227]; Chandra Fellowship Program
[PF6-70043]; NSF [AST-0805832]; Smithsonian Endowment Funds
FX We thank an anonymous referee for very helpful comments and a thorough
reading of our paper. J. E. M. acknowledges support from NASA grant
NNX08AJ55G. J. F. L. acknowledges support provided by NASA through grant
HST-GO-11227 and the Chandra Fellowship Program, grant PF6-70043. R. N.
acknowledges support from NASA grant NNX08AH32G and NSF grant
AST-0805832. J. F. S. was supported by the Smithsonian Endowment Funds.
S. W. D. acknowledges support through the Chandra Fellowship Program,
grant PF6-70043. R. A. R. acknowledges support from the NASA contract to
MIT for the instrument team contributing to RXTE. This research has made
use of data obtained from the High Energy Astrophysics Science Archive
Research Center ( HEASARC) at NASA/Goddard Space Flight Center.
NR 64
TC 59
Z9 59
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1076
EP 1090
DI 10.1088/0004-637X/701/2/1076
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500017
ER
PT J
AU Irwin, J
Charbonneau, D
Berta, ZK
Quinn, SN
Latham, DW
Torres, G
Blake, CH
Burke, CJ
Esquerdo, GA
Furesz, G
Mink, DJ
Nutzman, P
Szentgyorgyi, AH
Calkins, ML
Falco, EE
Bloom, JS
Starr, DL
AF Irwin, Jonathan
Charbonneau, David
Berta, Zachory K.
Quinn, Samuel N.
Latham, David W.
Torres, Guillermo
Blake, Cullen H.
Burke, Christopher J.
Esquerdo, Gilbert A.
Furesz, Gabor
Mink, Douglas J.
Nutzman, Philip
Szentgyorgyi, Andrew H.
Calkins, Michael L.
Falco, Emilio E.
Bloom, Joshua S.
Starr, Dan L.
TI GJ 3236: A NEW BRIGHT, VERY LOW MASS ECLIPSING BINARY SYSTEM DISCOVERED
BY THE MEARTH OBSERVATORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; stars: individual (GJ 3236); stars: low-mass, brown
dwarfs
ID STELLAR ATMOSPHERE MODELS; ORION NEBULA CLUSTER; LIMB-DARKENING LAW;
URSA-MAJOR GROUP; ABSOLUTE DIMENSIONS; MAIN-SEQUENCE; M-DWARFS;
EVOLUTIONARY MODELS; CM DRACONIS; SURFACE GRAVITIES
AB We report the detection of eclipses in GJ 3236, a bright (I = 11.6), very low mass binary system with an orbital period of 0.77 days. Analysis of light and radial velocity curves of the system yielded component masses of 0.38 +/- 0.02 M circle dot and 0.28 +/- 0.02 M circle dot. The central values for the stellar radii are larger than the theoretical models predict for these masses, in agreement with the results for existing eclipsing binaries, although the present 5% observational uncertainties limit the significance of the larger radii to approximately 1 sigma. Degeneracies in the light curve models resulting from the unknown configuration of surface spots on the components of GJ 3236 currently dominate the uncertainties in the radii, and could be reduced by obtaining precise, multiband photometry covering the full orbital period. The system appears to be tidally synchronized and shows signs of high activity levels as expected for such a short orbital period, evidenced by strong Ha emission lines in the spectra of both components. These observations probe an important region of mass-radius parameter space around the predicted transition to fully convective stellar interiors, where there are a limited number of precise measurements available in the literature.
C1 [Irwin, Jonathan; Charbonneau, David; Berta, Zachory K.; Quinn, Samuel N.; Latham, David W.; Torres, Guillermo; Blake, Cullen H.; Burke, Christopher J.; Esquerdo, Gilbert A.; Furesz, Gabor; Mink, Douglas J.; Nutzman, Philip; Szentgyorgyi, Andrew H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Calkins, Michael L.; Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bloom, Joshua S.; Starr, Dan L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Irwin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jirwin@cfa.harvard.edu
OI Berta-Thompson, Zachory/0000-0002-3321-4924; Mink,
Jessica/0000-0003-3594-1823; Charbonneau, David/0000-0002-9003-484X
FU David and Lucile Packard Fellowship for Science and Engineering;
National Science Foundation [AST-0807690]; NASA Kepler mission
[NCC2-1390]; NSF [AST-0708229]; NASA; NSF; NASA's Astrophysics Data
System; SIMBAD database; CDS, Strasbourg, France; U. S. Government
[W-2166]; Harvard University Milton Fund; University of Virginia;
NASA/Swift Guest Investigator [NNG06GH50G]; PAIRITEL project
FX This research has made extensive use of data products from the Two
Micron All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by NASA and the NSF, NASA's Astrophysics
Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg,
France. The Digitized Sky Surveys were produced at the Space Telescope
Science Institute under U. S. Government grant NAG W-2166. The images of
these surveys are based on photographic data obtained using the Oschin
Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The
plates were processed into the present compressed digital form with the
permission of these institutions. The Peters Automated Infrared Imaging
Telescope (PAIRITEL) is operated by the Smithsonian Astrophysical
Observatory (SAO) and was made possible by a grant from the Harvard
University Milton Fund, the camera loan from the University of Virginia,
and the continued support of the SAO and U. C. Berkeley. The PAIRITEL
project and J.S.B. are further supported by NASA/Swift Guest
Investigator Grant NNG06GH50G. We thank M. Skrutskie for his continued
support of the PAIRITEL project.
NR 65
TC 44
Z9 46
U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1436
EP 1449
DI 10.1088/0004-637X/701/2/1436
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500043
ER
PT J
AU Flagey, N
Noriega-Crespo, A
Boulanger, F
Carey, SJ
Brooke, TY
Falgarone, E
Huard, TL
McCabe, CE
Miville-Deschenes, MA
Padgett, DL
Paladini, R
Rebull, LM
AF Flagey, N.
Noriega-Crespo, A.
Boulanger, F.
Carey, S. J.
Brooke, T. Y.
Falgarone, E.
Huard, T. L.
McCabe, C. E.
Miville-Deschenes, M. A.
Padgett, D. L.
Paladini, R.
Rebull, L. M.
TI EVIDENCE FOR DUST EVOLUTION WITHIN THE TAURUS COMPLEX FROM SPITZER
IMAGES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: clouds; ISM: evolution; ISM:
individual (Taurus Molecular Complex)
ID MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY CAMERA; ABSOLUTE
CALIBRATION; INTERSTELLAR DUST; MOLECULAR CLOUD; STAR-FORMATION; MU-M;
PHOTODISSOCIATION REGIONS; ULTRAVIOLET EXTINCTION; OPTICAL-PROPERTIES
AB We present Spitzer images of the Taurus Complex (TC). We take advantage of the sensitivity and the spatial resolution of the observations to characterize the diffuse infrared ( IR) emission across the cloud. This work highlights evidence of dust evolution within the translucent sections of the archetype reference for studies of quiescent molecular clouds. We combine the Spitzer 160 mu m and IRAS 100 mu m observations to produce a dust temperature map and a far-IR (FIR) dust opacity map at 5 ' resolution. The average dust temperature is about 14.5 K with a dispersion of +/- 1 K across the cloud. The FIR dust opacity is tightly correlated with the extinction derived from Two Micron All Sky Survey stellar colors and is a factor of 2 larger than the average value for the diffuse interstellar medium. This opacity increase and the attenuation of the radiation field both contribute to account for the lower emission temperature of the large grains. The structure of the TC significantly changes in the mid-IR (MIR) images that trace emission from polycyclic aromatic hydrocarbons (PAHs) and very small grains (VSGs). We focus our analysis of the MIR emission to a range of ecliptic latitudes away from the zodiacal bands and where the zodiacal light residuals are small. Within this cloud area, there are no 8 and 24 mu m counterparts to the brightest 160 mu m emission features. Conversely, the 8 and 24 mu m images reveal filamentary structure that is strikingly inconspicuous in the 160 mu m and extinction maps. The IR colors vary over subparsec distances across this filamentary structure. We compare the observed colors with model calculations quantifying the impact of the radiation field intensity and the abundance of stochastically heated particles on the dust spectral energy distribution. To match the range of observed colors, we have to invoke variations by a factor of a few of both the interstellar radiation field and the abundance of PAHs and VSGs. We conclude that within this filamentary structure a significant fraction of the dust mass cycles in and out the small-size end of the dust size distribution.
C1 [Flagey, N.; Noriega-Crespo, A.; Carey, S. J.; Brooke, T. Y.; McCabe, C. E.; Padgett, D. L.; Paladini, R.; Rebull, L. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Flagey, N.; Boulanger, F.; Miville-Deschenes, M. A.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Falgarone, E.] Ecole Normale Super, LERMA LRA, CNRS UMR 8112, F-75231 Paris, France.
[Falgarone, E.] Observ Paris, F-75231 Paris 05, France.
[Huard, T. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[McCabe, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Flagey, N (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd,MC 220-6, Pasadena, CA 91125 USA.
EM nflagey@ipac.caltech.edu
OI Rebull, Luisa/0000-0001-6381-515X
FU Jet Propulsion Laboratory; California Institute of Technology
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.
NR 69
TC 31
Z9 31
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1450
EP 1463
DI 10.1088/0004-637X/701/2/1450
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500044
ER
PT J
AU O'Sullivan, E
Giacintucci, S
Vrtilek, JM
Raychaudhury, S
David, LP
AF O'Sullivan, E.
Giacintucci, S.
Vrtilek, J. M.
Raychaudhury, S.
David, L. P.
TI A CHANDRA X-RAY VIEW OF STEPHAN'S QUINTET: SHOCKS AND STAR FORMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (Stephan's Quintet, HCG 92); galaxies:
interactions; intergalactic medium; X-rays: galaxies
ID RADIO-CONTINUUM EMISSION; FORMATION RATE INDICATOR; INTRAGROUP MEDIUM;
GALAXY COLLISION; MULTIWAVELENGTH; REGIONS; CLUSTER; GAS
AB We use a deep Chandra observation to examine the structure of the hot intra-group medium of the compact group of galaxies Stephan's Quintet. The group is thought to be undergoing a strong dynamical interaction as an interloper, NGC 7318b, passes through the group core at similar to 850 km s(-1). Previous studies have interpreted a bright ridge of X-ray and radio continuum emission as the result of shock heating, with support from observations at other wavelengths. We find that gas in this ridge has a similar temperature (similar to 0.6 keV) and abundance (similar to 0.3 Z(circle dot)) to the surrounding diffuse emission, and that a hard emission component is consistent with that expected from high-mass X-ray binaries associated with star formation in the ridge. The cooling rate of gas in the ridge is consistent with the current star formation rate, suggesting that radiative cooling is driving the observed star formation. The lack of a high-temperature gas component is used to place constraints on the nature of the interaction and shock, and we find that an oblique shock heating a pre-existing. lament of Hi may be the most likely explanation of the X-ray gas in the ridge. The mass of hot gas in the group is roughly equal to the deficit in observed Hi mass compared to predictions, but only similar to 2% of the gas is contained in the ridge. The hot gas component is too extended to have been heated by the current interaction, strongly suggesting that it must have been heated during previous dynamical encounters.
C1 [O'Sullivan, E.; Giacintucci, S.; Vrtilek, J. M.; David, L. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM eosullivan@cfa.harvard.edu
OI O'Sullivan, Ewan/0000-0002-5671-6900
FU National Aeronautics and Space Administration through Chandra Award
[G07-8133X-R]; National Aeronautics Space Administration [NAS8-03060]
FX The authors thank S. Immler and D. J. Saikia for providing access to the
Swift and GMRT data, and P. Nulsen, A. Zezas, and T. J. Ponman for
helpful discussion of various aspects of the paper. Support for this
work was provided by the National Aeronautics and Space Administration
through Chandra Award Number G07-8133X-R 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. This research has made use of
software provided by the Chandra X-ray Center (CXC) in the application
packages CIAO, ChIPS, and Sherpa, and of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 33
TC 24
Z9 24
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1560
EP 1568
DI 10.1088/0004-637X/701/2/1560
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500053
ER
PT J
AU Blocker, AW
Protopapas, P
Alcock, CR
AF Blocker, Alexander W.
Protopapas, Pavlos
Alcock, Charles R.
TI A BAYESIAN APPROACH TO THE ANALYSIS OF TIME SYMMETRY IN LIGHT CURVES:
RECONSIDERING SCORPIUS X-1 OCCULTATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Kuiper Belt; methods: data analysis; methods: numerical; methods:
statistical; stars: individual (Scorpius X-1)
ID KUIPER-BELT OBJECTS; STELLAR OCCULTATIONS; SIZE DISTRIBUTION;
MILLISECOND DIPS; SCO X-1; BODIES; SEARCH; STARS
AB We present a new approach to the analysis of time symmetry in light curves, such as those in the X-ray at the center of the Scorpius X-1 occultation debate. Our method uses a new parameterization for such events (the bilogistic event profile) and provides a clear, physically relevant characterization of each event's key features. We also demonstrate a Markov chain Monte Carlo algorithm to carry out this analysis, including a novel independence chain configuration for the estimation of each event's location in the light curve. These tools are applied to the Scorpius X-1 light curves presented in Chang et al., providing additional evidence based on the time series that the events detected thus far are most likely not occultations by trans-Neptunian objects.
C1 [Blocker, Alexander W.] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA.
[Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Protopapas, Pavlos; Alcock, Charles R.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA.
RP Blocker, AW (reprint author), Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA.
FU NSF [AST0501681]; Harvard FAS Research Computing Group
FX We gratefully acknowledge the support from NSF AST0501681. We also thank
the participants in the Harvard Astrostatistics Seminar for their
feedback, particularly Xiao-Li Meng. The simulations in this paper were
run on the Odyssey cluster supported by the Harvard FAS Research
Computing Group.
NR 25
TC 3
Z9 3
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1742
EP 1752
DI 10.1088/0004-637X/701/2/1742
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500068
ER
PT J
AU Marchesini, D
van Dokkum, PG
Schreiber, NMF
Franx, M
Labbe, I
Wuyts, S
AF Marchesini, Danilo
van Dokkum, Pieter G.
Schreiber, Natascha M. Foerster
Franx, Marijn
Labbe, Ivo
Wuyts, Stijn
TI THE EVOLUTION OF THE STELLAR MASS FUNCTION OF GALAXIES FROM z=4.0 AND
THE FIRST COMPREHENSIVE ANALYSIS OF ITS UNCERTAINTIES: EVIDENCE FOR
MASS-DEPENDENT EVOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: distances and redshifts; galaxies: evolution; galaxies:
formation; galaxies: fundamental parameters; galaxies: high-redshift;
galaxies: luminosity function, mass function; galaxies: stellar content;
infrared: galaxies
ID HIGH-REDSHIFT GALAXIES; DEEP FIELD-SOUTH; SPITZER-SPACE-TELESCOPE;
INFRARED ARRAY CAMERA; STAR-FORMING GALAXIES; OPTICAL LUMINOSITY
FUNCTIONS; ACTIVE GALACTIC NUCLEI; SMALL MAGELLANIC CLOUD; GOODS-MUSIC
SAMPLE; YALE-CHILE MUSYC
AB We present the evolution of the stellar mass function (SMF) of galaxies from z = 4.0 to z = 1.3 measured from a sample constructed from the deep near-infrared Multi-wavelength Survey by Yale-Chile, the Faint Infrared Extragalactic Survey, and the Great Observatories Origins Deep Survey-Chandra Deep Field South surveys, all having very high-quality optical to mid-infrared data. This sample, unique in that it combines data from surveys with a large range of depths and areas in a self-consistent way, allowed us to (1) minimize the uncertainty due to cosmic variance and empirically quantify its contribution to the total error budget; (2) simultaneously probe the high-mass end and the low-mass end (down to similar to 0.05 times the characteristic stellar mass) of the SMF with good statistics; and (3) empirically derive the redshift-dependent completeness limits in stellar mass. We provide, for the first time, a comprehensive analysis of random and systematic uncertainties affecting the derived SMFs, including the effect of metallicity, extinction law, stellar population synthesis model, and initialmass function. We find that the mass density evolves by a factor of similar to 17(-10)(+7) since z = 4.0, mostly driven by a change in the normalization Phi(star). If only random errors are taken into account, we find evidence for mass-dependent evolution, with the low-mass end evolving more rapidly than the high-mass end. However, we show that this result is no longer robust when systematic uncertainties due to the SED-modeling assumptions are taken into account. Another significant uncertainty is the contribution to the overall stellar mass density of galaxies below our mass limit; future studies with WFC3 will provide better constraints on the SMF at masses below 10(10) M(circle dot) at z > 2. Taking our results at face value, we find that they are in conflict with semianalytic models of galaxy formation. The models predict SMFs that are in general too steep, with too many low-mass galaxies and too few high-mass galaxies. The discrepancy at the high-mass end is susceptible to uncertainties in the models and the data, but the discrepancy at the low-mass end may be more difficult to explain.
C1 [Marchesini, Danilo; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Schreiber, Natascha M. Foerster] MPE, D-85748 Garching, Germany.
[Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Labbe, Ivo] Carnegie Observ, Pasadena, CA 91101 USA.
[Wuyts, Stijn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Marchesini, D (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
EM danilo.marchesini@yale.edu
FU AURA, Inc.; NASA [NAS5-26555]; European Southern Observatories, Chile
[LP164.O-0612, 168.A-0485, 170.A-0788, 074.A-0709, 275.A-5060,
171.A-3045]; National Science Foundation
FX Based on observations with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory (JPL), California Institute of
Technology under NASA contract 1407. 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
NAS5-26555. Based on observations collected at the European Southern
Observatories, Chile (ESO Programme LP164.O-0612, 168.A-0485,
170.A-0788, 074.A-0709, 275.A-5060, and 171.A-3045). Based on
observations obtained at the Cerro Tololo Inter-American Observatory, a
division of the National Optical Astronomy Observatories, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under cooperative agreement with the National Science Foundation.
NR 100
TC 316
Z9 316
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1765
EP 1796
DI 10.1088/0004-637X/701/2/1765
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500070
ER
PT J
AU Kennea, JA
Mukai, K
Sokoloski, JL
Luna, GJM
Tueller, J
Markwardt, CB
Burrows, DN
AF Kennea, J. A.
Mukai, K.
Sokoloski, J. L.
Luna, G. J. M.
Tueller, J.
Markwardt, C. B.
Burrows, D. N.
TI SWIFT OBSERVATIONS OF HARD X-RAY EMITTING WHITE DWARFS IN SYMBIOTIC
STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE white dwarfs; X-rays: binaries; X-rays: stars
ID T-CORONAE-BOREALIS; CH-CYGNI; CATACLYSMIC VARIABLES; BINARY-SYSTEM;
R-AQUARII; SS-CYGNI; EMISSION; JET; TELESCOPE; VARIABILITY
AB The X-ray emission from most accreting white dwarfs (WDs) in symbiotic binary stars is quite soft. Several symbiotic WDs, however, produce strong X-ray emission at energies greater than similar to 20 keV. The Swift Burst Alert Telescope (BAT) instrument has detected hard X-ray emission from four such accreting WDs in symbiotic stars: RT Cru, T CrB, CD -57 3057, and CH Cyg. In one case (RT Cru), Swift detected X-rays out to greater than 50 keV at > 5 sigma confidence level. Combining data from the X-Ray Telescope (XRT) and BAT detectors, we find that the 0.3-150 keV spectra of RT Cru, T CrB, and CD -57 3057 are well described by emission from a single-temperature, optically thin thermal plasma, plus an unresolved 6.4-6.9 keV Fe line complex. The X-ray spectrum of CH Cyg contains an additional bright soft component. For all four systems, the spectra suffer high levels of absorption from material that both fully and partially covers the source of hard X-rays. The XRT data did not show any of the rapid, periodic variations that one would expect if the X-ray emission were due to accretion onto a rotating, highly magnetized WD. The X-rays were thus more likely from the accretion-disk boundary layer around a massive, non-magnetic WD in each binary. The X-ray emission from RT Cru varied on timescales of a few days. This variability is consistent with being due to changes in the absorber that partially covers the source, suggesting localized absorption from a clumpy medium moving into the line of sight. The X-ray emission from CD -57 3057 and T CrB also varied during the nine months of Swift observations, in a manner that was also consistent with variable absorption.
C1 [Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Mukai, K.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, K.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Luna, G. J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Markwardt, C. B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Kennea, JA (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Tueller, Jack/D-5334-2012
FU NASA [NAS5-00136, NNX06AI16G, NNX08AG28G]
FX We thank the anonymous referee for their helpful comments and very
careful reading of the manuscript. This work is supported at Penn State
by NASA contract NAS5-00136 and at Columbia by NASA grants NNX06AI16G
and NNX08AG28G.
NR 53
TC 21
Z9 21
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 1992
EP 2001
DI 10.1088/0004-637X/701/2/1992
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500085
ER
PT J
AU Smith, RK
Chen, GX
Kirby, K
Brickhouse, NS
AF Smith, Randall K.
Chen, Guo-Xin
Kirby, Kate
Brickhouse, Nancy S.
TI A NEW CALCULATION OF Ne IX LINE DIAGNOSTICS (vol 700, pg 679, 2009)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Smith, Randall K.; Chen, Guo-Xin; Kirby, Kate; Brickhouse, Nancy S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rsmith@cfa.harvard.edu
NR 2
TC 2
Z9 2
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2009
VL 701
IS 2
BP 2034
EP 2034
DI 10.1088/0004-637X/701/2/2034
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480UE
UT WOS:000268761500089
ER
PT J
AU Steiner, JF
McClintock, JE
Remillard, RA
Narayan, R
Gou, LJ
AF Steiner, James F.
McClintock, Jeffrey E.
Remillard, Ronald A.
Narayan, Ramesh
Gou, Lijun
TI MEASURING BLACK HOLE SPIN VIA THE X-RAY CONTINUUM-FITTING METHOD: BEYOND
THE THERMAL DOMINANT STATE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; stars: individual
(H1743-322, XTE J1550-564); X-rays: binaries
ID ACCRETION DISK; MICROQUASAR XTE-J1550-564; TIMING-EXPLORER; XTE
J1550-564; BINARIES; COMPTONIZATION; SPECTROSCOPY; MCG-6-30-15;
CALIBRATION; OUTBURST
AB All prior work on measuring the spins of stellar-mass black holes (BHs) via the X-ray continuum-fitting (CF) method has relied on the use of weakly Comptonized spectra obtained in the thermal dominant (TD) state. Using a self-consistent Comptonization model, we show that one can analyze spectra that exhibit strong power-law components and obtain values of the inner disk radius, and hence spin, that are consistent with those obtained in the TD state. Specifically, we analyze many RXTE spectra of two BH transients, H1743-322 and XTE J1550-564, and we demonstrate that the radius of the inner edge of the accretion disk remains constant to within a few percent as the strength of the Comptonized component increases by an order of magnitude, i.e., as the fraction of the thermal seed photons that are scattered approaches 25%. We conclude that the CF method can be applied to a much wider body of data than previously thought possible, and to sources that have never been observed to enter the TD state (e.g., Cyg X-1).
C1 [Steiner, James F.; McClintock, Jeffrey E.; Narayan, Ramesh; Gou, Lijun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jsteiner@cfa.harvard.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU Smithsonian Institution Endowment Funds; NASA [NNX08AJ55G, NNX08AH32G];
NSF [AST-0805832]
FX The authors thank Jifeng Liu for valuable discussions. J.F.S. was
supported by the Smithsonian Institution Endowment Funds and J.E.M.
acknowledges support from NASA grant NNX08AJ55G. R.N. acknowledges
support from NASA grant NNX08AH32G and NSF grant AST-0805832. R. A. R.
acknowledges partial support from the NASA contract to MIT for support
of RXTE instruments.
NR 26
TC 52
Z9 54
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2009
VL 701
IS 2
BP L83
EP L86
DI 10.1088/0004-637X/701/2/L83
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482ET
UT WOS:000268867900005
ER
PT J
AU Lee, MY
Munroe, TA
Chen, HM
AF Lee, Mao-Ying
Munroe, Thomas A.
Chen, Hong-Ming
TI A new species of tonguefish (Pleuronectiformes: Cynoglossidae) from
Taiwanese waters
SO ZOOTAXA
LA English
DT Article
DE Symphurus; flatfish; deep waters; systematics; Pepperdot tonguefish
ID SYMPHURUS CYNOGLOSSIDAE; PACIFIC; OCEAN
AB Symphurus multimaculatus new species, described from nine specimens captured in deep waters off Taiwan, is distinguished from congeners by the following combination of characters: predominant 1-2-2-2-2 pattern of interdigitation of dorsal pterygiophores and neural spines, 14 caudal-fin rays, 92-94 dorsal-fin rays, 79-82 anal-fin rays, 9 abdominal and 50-51 total vertebrae, 5 hypurals, deep body (28.6-35.1 % SL), small scales (102-108 scales in longitudinal series, 45-48 scales in transverse row), blackish-brown ocular-side opercle, bluish-black blind-side opercle, uniformly reddish-brown to dark-brown ocular-side background pigmentation with some specimens also having 5-7 mostly complete crossbands, and uniformly white to light-yellow blind side with dense patches of blackish-brown chromatophores predominantly covering pterygiophore regions of the dorsal and anal fins. Symphurus multimaculatus were retrieved from commercial catches of fishing trawlers landed at three regional fish ports operating in deep waters off northeastern and southwestern Taiwan. The only information associated with these specimens is the general region of capture based on where fishing trawlers operate. Data on relative abundance, depth of capture, geographic distribution, and microhabitat conditions where this species is captured are unavailable at this time.
C1 [Lee, Mao-Ying] Acad Sinica, Biodivers Res Ctr, Lab Fish Ecol & Evolut, Taipei 11529, Taiwan.
[Munroe, Thomas A.] Smithsonian Inst, NOAA, Natl Marine Fisheries Serv, Natl Museum Nat Hist,Natl Systemat Lab, Washington, DC 20013 USA.
[Lee, Mao-Ying; Chen, Hong-Ming] Natl Taiwan Ocean Univ, Dept Aquaculture, Chilung 20224, Taiwan.
RP Lee, MY (reprint author), Acad Sinica, Biodivers Res Ctr, Lab Fish Ecol & Evolut, Taipei 11529, Taiwan.
EM coleopetera@gmail.com; munroet@si.edu; hmchen@mail.ntou.edu.tw
FU National Science Council [NSC 92-2311-B-001-034]; Biodiversity Research
Center, Academia Sinica
FX This work represents a portion of collecting activities investigating
the biodiversity of deep-sea fishes in Taiwanese waters supported
through a grant (NSC 92-2311-B-001-034) from the National Science
Council to K.-T. Shao, Biodiversity Research Center, Academia Sinica. We
thank H.-C. Ho, P.-F. Lee and Y.-C. Liao for help in collecting
specimens and for kindly providing other specimens used in this study.
L.-P. Lin assisted with loans and shipments of specimens. M. Nizinski
provided assistance and support during M.-Y. Lee's visit to the National
Museum of Natural History, Smithsonian Institution. J. Williams, J.
Clayton, R. Vari and L. Parenti provided assistance with specimens in
their care. M.-Y. Lee extends his appreciation to members of the
Laboratory of Fish Ecology and Evolution for their support and
assistance during this study. We extend our appreciation to all curators
and researchers who provided specimens, loans and other materials that
benefited this study.
NR 29
TC 7
Z9 8
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 AUG 19
PY 2009
IS 2203
BP 49
EP 58
PG 10
WC Zoology
SC Zoology
GA 485VS
UT WOS:000269153500004
ER
PT J
AU Volkov, I
Banavar, JR
Hubbell, SP
Maritan, A
AF Volkov, Igor
Banavar, Jayanth R.
Hubbell, Stephen P.
Maritan, Amos
TI Inferring species interactions in tropical forests
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE ecology; maximum entropy principle; stochastic
ID MAXIMUM-ENTROPY PRODUCTION; INFORMATION-THEORY; STATISTICAL MECHANICS;
FLUCTUATION THEOREM; ABUNDANCE; PATTERNS; ECOLOGY; BIODIVERSITY;
DIVERSITY; STATES
AB We present 2 distinct and independent approaches to deduce the effective interaction strengths between species and apply it to the 20 most abundant species in the long-term 50-ha plot on Barro Colorado Island, Panama. The first approach employs the principle of maximum entropy, and the second uses a stochastic birth-death model. Both approaches yield very similar answers and show that the collective effects of the pairwise interspecific interaction strengths are weak compared with the intraspecific interactions. Our approaches can be applied to other ecological communities in steady state to evaluate the extent to which interactions need to be incorporated into theoretical explanations for their structure and dynamics.
C1 [Volkov, Igor; Banavar, Jayanth R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Volkov, Igor] Penn State Univ, Dept Biol, Mueller Lab, University Pk, PA 16802 USA.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa, Ancon Panama, Panama.
[Maritan, Amos] Univ Padua, Dipartimento Fis G Galilei, Consorzio Nazl Interuniv Sci Fis Mat, Ist Nazl Fis Nucl, I-35131 Padua, Italy.
RP Banavar, JR (reprint author), Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
EM jayanth@phys.psu.edu; amos.maritan@pd.infn.it
FU Cariparo Foundation
FX We are grateful to Jim Brown for insightful advice, Tim Lezon for useful
discussions, and 2 anonymous reviewers for carefully reading our paper
and making important suggestions. This work was supported by the
Cariparo Foundation.
NR 32
TC 38
Z9 42
U1 5
U2 31
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 18
PY 2009
VL 106
IS 33
BP 13854
EP 13859
DI 10.1073/pnas.0903244106
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 484WE
UT WOS:000269078700043
PM 19666524
ER
PT J
AU Macdonald, KS
Hultgren, K
Duffy, JE
AF Macdonald, Kenneth S., III
Hultgren, Kristin
Duffy, J. Emmett
TI The sponge-dwelling snapping shrimps (Crustacea, Decapoda, Alpheidae,
Synalpheus) of Discovery Bay, Jamaica, with descriptions of four new
species
SO ZOOTAXA
LA English
DT Article
DE Synalpheus; Zuzalpheus; gambarelloides group; Alpheidae; Decapoda;
symbiotic; coral reef; eusociality; sponges
ID BELIZE BARRIER-REEF; HOST-SPECIFICITY; SHALLOW-WATER; CORAL REEFS;
ZUZALPHEUS; RADIATION; ECOLOGY; MEXICO; FAUNA; GULF
AB Twenty-two species of sponge-dwelling shrimp in the genus Synalpheus were collected in the vicinity of Discovery Bay, Jamaica. Four of these species are new to science. Synalpheus thele n.sp., S. corallinus n. sp., and S. plumosetosus n. sp. belong to a group of morphologically similar species that also includes S. brooksi, S. bousfieldi, S. carpenteri, and S. chacei. Synalpheus irie n. sp. is a highly distinctive shrimp most similar to S. mcclendoni, but can be distinguished from the latter by the unique bowl-shaped fingers of the major chela and the two-pronged distal protuberance on the palm of the major chela. Synalpheus belizensis and S. regalis are reported for the first time from outside their type localities in Belize, while S. bocas and S. duffyi are reported for the first time outside their type localities in Caribbean Panama.
C1 [Macdonald, Kenneth S., III] New Mexico State Univ, Dept Fish Wildlife & Conservat Ecol, Las Cruces, NM 88003 USA.
[Hultgren, Kristin] Smithsonian Trop Res Inst, Naos Lab, Balboa Ancon, Panama.
[Duffy, J. Emmett] Coll William & Mary, Sch Marine Sci, Williamsburg, VA 23187 USA.
[Duffy, J. Emmett] Coll William & Mary, Virginia Inst Marine Sci, Williamsburg, VA 23187 USA.
RP Macdonald, KS (reprint author), New Mexico State Univ, Dept Fish Wildlife & Conservat Ecol, Las Cruces, NM 88003 USA.
EM tripp@nmsu.edu; hultgrenk@si.edu; jeduffy@vims.edu
RI Macdonald, Kenneth/F-9822-2011
FU The National Geographic Society [831-207]; Smithsonian Marine Science
Network
FX We are grateful to Anthony Downes, Peter Gayle, and the staff of the
Discovery Bay Marine Lab for facilitating our field research, and to the
Jamaica National Environment and Planning Agency for permission to
collect and export specimens. The National Geographic Society (Research
and Exploration Grant #831-207) and the Smithsonian Marine Science
Network provided financial support. We are also grateful to Arthur Anker
for his thorough review of this manuscript. This is VIMS contribution
no. 3030.
NR 60
TC 18
Z9 21
U1 4
U2 5
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD AUG 17
PY 2009
IS 2199
BP 1
EP 57
PG 57
WC Zoology
SC Zoology
GA 483UC
UT WOS:000268992700001
ER
PT J
AU Turner, BL
AF Turner, Benjamin L.
TI Chemistry and dynamics of organic phosphorus in the environment
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
C1 [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
EM TurnerBL@si.edu
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
NR 0
TC 0
Z9 0
U1 2
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 16
PY 2009
VL 238
MA 16-AGRO
BP 591
EP 591
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA V16HY
UT WOS:000207861900551
ER
PT J
AU Atkins, TM
Cassidy, MC
Mair, RW
Walsworth, RL
Marcus, CM
Kauzlarich, SM
AF Atkins, Tonya M.
Cassidy, Maja C.
Mair, R. W.
Walsworth, R. L.
Marcus, C. M.
Kauzlarich, Susan M.
TI Synthesis of silicon nanoparticles for hyperpolarized magnetic resonance
imaging
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
C1 [Atkins, Tonya M.; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA.
[Cassidy, Maja C.; Mair, R. W.; Marcus, C. M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM tmatkins@ucdavis.edu
RI Marcus, Charles/M-4526-2014
OI Marcus, Charles/0000-0003-2420-4692
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 16
PY 2009
VL 238
MA 851-INOR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA V16HZ
UT WOS:000207862000792
ER
PT J
AU Koestler, RJ
DePriest, PT
AF Koestler, Robert J.
DePriest, Paula T.
TI COLL 460-Keynote Address. Lascaux's mold: Repainting the art
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
C1 [Koestler, Robert J.; DePriest, Paula T.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
EM KoestlerR@si.edu; DepriestP@si.edu
RI DePriest, Paula/K-6633-2015
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 16
PY 2009
VL 238
MA 460-COLL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA V16HY
UT WOS:000207861903544
ER
PT J
AU Head, JW
Murchie, SL
Prockter, LM
Solomon, SC
Chapman, CR
Strom, RG
Watters, TR
Blewett, DT
Gillis-Davis, JJ
Fassett, CI
Dickson, JL
Morgan, GA
Kerber, L
AF Head, James W.
Murchie, Scott L.
Prockter, Louise M.
Solomon, Sean C.
Chapman, Clark R.
Strom, Robert G.
Watters, Thomas R.
Blewett, David T.
Gillis-Davis, Jeffrey J.
Fassett, Caleb I.
Dickson, James L.
Morgan, Gareth A.
Kerber, Laura
TI Volcanism on Mercury: Evidence from the first MESSENGER flyby for
extrusive and explosive activity and the volcanic origin of plains
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; volcanism; plains; Caloris basin; MESSENGER
ID SOUTH-POLE-AITKEN; OCEANUS-PROCELLARUM; TRANSPORT MECHANISMS; ERUPTION
CONDITIONS; CRATERING RECORD; LUNAR VOLCANISM; IMPACT CRATERS; MARE
DEPOSITS; STRATIGRAPHY; BASINS
AB The first MESSENGER flyby of Mercury obtained images of 21% of the surface not seen by Mariner 10, including the center and western half of the Caloris basin and regions near the terminator that show details of the nature of smooth and intercrater plains. These new data have helped to address and resolve a series of longstanding questions on the existence and nature of volcanism on Mercury and the distribution of volcanic materials. Data from the Mercury Dual Imaging System (MDIS) on the MESSENGER spacecraft have shown the following: (1) Numerous volcanic vents, in the form of irregularly shaped rimless depressions, are concentrated around the interior edge of the Caloris basin. (2) These vents appear to be sources for effusive volcanism that in one case built a shield in excess of 100 km in diameter and in some cases formed bright haloes around the vents that are interpreted to represent pyroclastic eruptions. (3) Lobate margins of plains units, seen previously in Mariner 10 data, are documented in MESSENGER images with more clarity and are often distinctive in morphology and color properties, supporting the interpretation that these features are the edges of lava flow units. (4) The interior of the Caloris basin is filled with plains units spectrally distinctive from the rim deposits, and comparison with the lunar Imbrium basin and superposed impact crater stratigraphy provide evidence that these units are volcanic in origin: detailed differences in the mineralogy of lava flow units, so prominent in Imbrium, are not seen in the Caloris interior. (5) Some of the smooth plains surrounding the exterior of the Caloris basin show distinct differences in color and morphological properties, supporting a volcanic origin. (6) Some smooth and intercrater plains units distant from the Caloris basin show evidence of flooding and embayment relations unrelated to Caloris ejecta emplacement; local and regional geological and color relationships support a volcanic origin for these plains. (7) Large impact craters show a sequence of embayment of interior floor and exterior ejecta deposits that supports a volcanic origin for the embayment and filling processes. (8) Crater embayment and flooding relationships in selected areas suggest volcanic plains thicknesses of many hundreds of meters and local thicknesses inside impact craters of up to several kilometers. (9) Impact crater size-frequency distributions for Caloris exterior deposits, including the facies of the Caloris Group and relatively high- and low-albedo smooth plains, show that they are younger than plains interior to Caloris and thus must be dominantly the product of post-Caloris volcanism. These new data provide evidence that supports and confirms earlier hypotheses from Mariner 10 data that volcanism was important in shaping the surface of Mercury. The emerging picture of the volcanic style of Mercury is similar to that of the Moon, the other small, one-plate planetary body: there are no major shield volcanoes (e.g., comparable to Tharsis Montes on Mars), shallow magma reservoirs are rare, and there is little evidence for surface deformation or long-lived volcanic sources related to sites of upwelling mantle. The close association of volcanic plains and surface deformation features suggests that future observations and analyses can help document the relation between the volcanic flux and the evolving state and magnitude of stress in the lithosphere of Mercury. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Head, James W.; Fassett, Caleb I.; Dickson, James L.; Morgan, Gareth A.; Kerber, Laura] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Murchie, Scott L.; Prockter, Louise M.; Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA.
[Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
RP Head, JW (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM James_Head_lll@Brown.edu
RI Murchie, Scott/E-8030-2015;
OI Murchie, Scott/0000-0002-1616-8751; Fassett, Caleb/0000-0001-9155-3804
FU NASA [NASW-00002, NAS5-97271]
FX We gratefully acknowledge the personnel of the Johns Hopkins University
Applied Physics Laboratory, who have planned and executed the MESSENGER
mission. Without their dedication and perseverance, this analysis would
not have been possible. We thank Kris Becker, Mark Robinson, Brett
Denevi, and all those who worked long and hard to process and calibrate
the MDIS data. The careful reviews by Mark Cintala and an unidentified
reviewer helped to improve the manuscript and are gratefully
acknowledged. The MESSENGER Project is supported by the NASA Discovery
Program under contracts NASW-00002 to the Carnegie Institution of
Washington and NAS5-97271 to the Johns Hopkins University Applied
Physics Laboratory.
NR 90
TC 62
Z9 62
U1 1
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 15
PY 2009
VL 285
IS 3-4
BP 227
EP 242
DI 10.1016/j.epsl.2009.03.007
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000002
ER
PT J
AU Head, JW
Murchie, SL
Prockter, LM
Solomon, SC
Strom, RG
Chapman, CR
Watters, TR
Blewett, DT
Gillis-Davis, JJ
Fassett, CI
Dickson, JL
Hurwitz, DM
Ostrach, LR
AF Head, James W.
Murchie, Scott L.
Prockter, Louise M.
Solomon, Sean C.
Strom, Robert G.
Chapman, Clark R.
Watters, Thomas R.
Blewett, David T.
Gillis-Davis, J. J.
Fassett, Caleb I.
Dickson, James L.
Hurwitz, Debra M.
Ostrach, Lillian R.
TI Evidence for intrusive activity on Mercury from the first MESSENGER
flyby
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; dikes; intrusion; graben; MESSENGER
ID FLOOR-FRACTURED CRATERS; VOLCANIC RIFT ZONES; SURFACE DEFORMATION;
GLOBAL DISTRIBUTION; DIKE EMPLACEMENT; REGIONAL STRESS; KILAUEA VOLCANO;
DYKE SWARMS; CONE-SHEETS; BETA-REGIO
AB Images from MESSENGER's first flyby of Mercury have shown convincing evidence for surface volcanism. Here we report on evidence in the new data for several features that are characterized by fractures and graben - rare features on a planet dominated by contractional deformation - that may be linked to intrusive activity. These features include: (I) A floor-fractured crater, interpreted to have been the site of laccolith-like sill intrusions; the feature is similar to some floor-fractured craters on the Moon and shows evidence for individual fractured dome-like uplifts on the floor. (2) A concentric complex of graben, observed inside the peak ring on the floor of the similar to 250-km-diameter Raditladi basin and associated with dark plains and possibly embayed by them; the feature may represent an unusual type of floor-fracturing associated with deeper intrusions and related ring dikes or cone sheets, or the graben may instead be the product of non-magmatic uplift of the basin floor. (3) A large radial graben swarm, Pantheon Fossae, located near the center of the Caloris basin, thus far unique on Mercury, and characterized by hundreds of individual graben segments ranging from similar to 5 km to similar to 110 km in length. In the nexus, graben crosscut one another and produce a local polygonal pattern; others curve away from the center as the nexus is approached. Two scales of graben length are observed; the radius of the dense radially symmetric plexus of graben is similar to 175 km, and a few graben extend to greater radial distances to the north and southwest out to distances that intersect with a ring of generally concentric graben around the outer basin floor. Two width scales of graben are observed; a large graben about 8 km wide emerges from the nexus and extends for - 100 km: most graben are less than half this width. Some graben walls appear cuspate, with convex-outward wall segments that resemble crater chain segments. One crater chain with distinctive raised rims parallels nearby graben. Locally, some graben appear in en echelon patterns, and smaller graben sometimes show cross-cutting (superposition) relationships. Abundant impact craters, the most prominent being Apollodorus, and secondary crater clusters and chains are superposed on the graben system; there is little evidence that craters greater than 5 km in diameter have been cut by a graben. This relation implies that the graben swarm formed soon after the emplacement of the Caloris floor plains. These graben are interpreted to be the surface expression of a radial dike swarm emanating from a subsurface magma reservoir. Similar features, in which the dikes contribute to a near-surface stress field that favors radial graben, are known on the Earth, Venus, and Mars. The location of Pantheon Fossae in the center of the Caloris basin suggests that formation of the radial graben structure is linked to basin evolution. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Head, James W.; Fassett, Caleb I.; Dickson, James L.; Hurwitz, Debra M.; Ostrach, Lillian R.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Murchie, Scott L.; Prockter, Louise M.; Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Gillis-Davis, J. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
RP Head, JW (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM James_Head@brown.edu
RI Murchie, Scott/E-8030-2015;
OI Murchie, Scott/0000-0002-1616-8751; Fassett, Caleb/0000-0001-9155-3804
FU NASA [NASW-00002, NAS5-97271]
FX We gratefully acknowledge the personnel of the Johns Hopkins University
Applied Physics Laboratory who have planned and executed the MESSENGER
mission. Without their dedication and perseverance, this analysis would
not have been possible. We gratefully acknowledge Kris Becker, Mark
Robinson, Brett Denevi, and all those who have processed and calibrated
the MDIS data. Thanks are extended to Wouter Bleeker and an unidentified
reviewer whose careful reviews improved the quality of the paper. The
MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory.
NR 78
TC 38
Z9 39
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 15
PY 2009
VL 285
IS 3-4
BP 251
EP 262
DI 10.1016/j.epsl.2009.03.008
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000004
ER
PT J
AU Watters, TR
Solomon, SC
Robinson, MS
Head, JW
Andre, SL
Hauck, SA
Murchie, SL
AF Watters, Thomas R.
Solomon, Sean C.
Robinson, Mark S.
Head, James W.
Andre, Sarah L.
Hauck, Steven A., II
Murchie, Scott L.
TI The tectonics of Mercury: The view after MESSENGER'S first flyby
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; MESSENGER; tectonics; lobate scarp; wrinkle ridge; graben
ID LOBATE SCARPS; GLOBAL TECTONICS; TERRESTRIAL PLANETS; DESPUN PLANET;
THRUST FAULTS; CALORIS BASIN; VOLCANISM; CONTRACTION; EVOLUTION; TROUGHS
AB During its first flyby of Mercury, MESSENGER imaged many tectonic landforms, most of which are contractional in nature and include lobate scarps, high-relief ridges, and wrinkle ridges. Wrinkle ridges are found on the smooth plains that partially fill the interior and surround the exterior of the Caloris basin and also on smooth plains that fill the interiors of smaller impact basins and larger craters. MESSENGER revealed a radial graben complex, Pantheon Fossae, nearly co-centered with the Caloris basin. Pantheon Fossae and a network of mostly basin-concentric graben in the outer portions of the Caloris basin interior form a pattern of extension not seen elsewhere on Mercury The first clear example of extensional faults outside of the Caloris basin has been documented on smooth plains inside the peak ring of the relatively young Raditladi basin. A map of the distribution of tectonic landforms imaged by MESSENGER and Mariner 10 shows that lobate scarps are the most widespread type of feature. Estimates of the horizontal shortening associated with lobate scarps that crosscut and overthrust small impact craters imaged by MESSENGER range from similar to 1 to 3 km. Previously unrecognized lobate scarps detected in areas imaged by Mariner 10 indicate that earlier estimates of contractional strain are low. A new estimate of the average areal contractional strain (similar to 0.06%) accommodated by scarps is at least one third greater than comparable previous estimates and corresponds to a decrease in Mercury's radius of at least 0.8 km since the end of heavy impact bombardment of the inner solar system. These figures are lower bounds because of the likelihood that not all lobate scarps have been identified even in areas imaged to date. Crosscutting and embayment relations revealed by MESSENGER suggest that lobate scarps formed before the end of smooth plains emplacement and continued to be active after the emplacement of the youngest smooth plains deposits. Relatively recent activity on lobate scarps may be the expression of slow but continuous radial contraction that accompanied cooling of Mercury's interior and the growth of the planet's solid inner core. Published by Elsevier B.V.
C1 [Watters, Thomas R.; Andre, Sarah L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Hauck, Steven A., II] Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
EM watterst@si.edu
RI Hauck, Steven/A-7865-2008; Murchie, Scott/E-8030-2015
OI Hauck, Steven/0000-0001-8245-146X; Murchie, Scott/0000-0002-1616-8751
FU NASA [NASW-00002, NAS5-97271]
FX We thank Matthew Golombek and Francis Nimmo for helpful comments that
improved the manuscript. The MESSENGER project is supported by the NASA
Discovery Program under contracts NASW-00002 to the Carnegie Institution
of Washington and NAS5-97271 to the Johns Hopkins University Applied
Physics Laboratory.
NR 40
TC 65
Z9 65
U1 1
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 15
PY 2009
VL 285
IS 3-4
BP 283
EP 296
DI 10.1016/j.epsl.2009.01.025
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000007
ER
PT J
AU Fassett, CI
Head, JW
Blewett, DT
Chapman, CR
Dickson, JL
Murchie, SL
Solomon, SC
Watters, TR
AF Fassett, Caleb I.
Head, James W.
Blewett, David T.
Chapman, Clark R.
Dickson, James L.
Murchie, Scott L.
Solomon, Sean C.
Watters, Thomas R.
TI Caloris impact basin: Exterior geomorphology, stratigraphy, morphometry,
radial sculpture, and smooth plains deposits
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; MESSENGER; Caloris basin; stratigraphy; smooth plains
ID MERCURIAN VOLCANISM; MESSENGER; ORIGIN; FLYBY; DICHOTOMY; SURFACE;
SYSTEM
AB The Mariner 10 flybys revealed the eastern third of the Caloris basin and demonstrated its importance as a chronostratigraphic marker for the geological history of Mercury. Uncertain after that mission were the size of the basin, the full distribution of materials deposited or modified during the impact process, and the stratigraphic and age relationships between Caloris and surrounding terrain. images obtained during MESSENGER's January 2008 flyby of Mercury revealed that the Caloris basin is similar to 15% larger than previously estimated and moderately elliptical (similar to 1525 by similar to 1315 km). Basin-related sculpture and secondary craters are dispersed widely in areas surrounding the basin, confirming the widespread significance of this event as a stratigraphic marker. Units mapped around Caloris on the basis of Mariner 10 data are generally recognized in regions observed for the first time by MESSENGER, including most facies of the Caloris Group (the Caloris Montes, Odin Formation, and Van Eyck Formation). The only unit without obvious exposures in MESSENGER images is the Nervo Formation, which was originally interpreted as impact melt or fallback ejecta. New measurements of the size-frequency distribution of impact craters both within the Caloris basin and on surrounding units, particularly the Odin Formation, support the hypothesis that the vast majority of circum-Caloris plains postdate the basin and are likely volcanic. The MESSENGER observations re-emphasize the importance of understanding the exterior stratigraphy of the basin in order to utilize the Caloris event as a discrete time horizon in the geological history of Mercury. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Fassett, Caleb I.; Head, James W.; Dickson, James L.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Blewett, David T.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
RP Fassett, CI (reprint author), Brown Univ, Dept Geol Sci, 324 Brook St,Box 1846, Providence, RI 02912 USA.
EM Caleb_Fassett@brown.edu
RI Murchie, Scott/E-8030-2015;
OI Murchie, Scott/0000-0002-1616-8751; Fassett, Caleb/0000-0001-9155-3804
FU NASA [NASW-00002, NAS5-97271]
FX We thank two anonymous reviewers, whose suggestions substantially
improved this contribution. We also acknowledge Debra Hurwitz, Laura
Kerber, Joe Levy, Gareth Morgan, and Sam Schon for their helpful
discussions. The MESSENGER Project is supported by the NASA Discovery
Program through contracts NASW-00002 with the Camegie Institution of
Washington and NAS5-97271 with the Johns Hopkins University Applied
Physics Laboratory.
NR 52
TC 45
Z9 45
U1 0
U2 5
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 AUG 15
PY 2009
VL 285
IS 3-4
SI SI
BP 297
EP 308
DI 10.1016/j.epsl.2009.05.022
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000008
ER
PT J
AU Watters, TR
Murchie, SL
Robinson, MS
Solomon, SC
Denevi, BW
Andre, SL
Head, JW
AF Watters, Thomas R.
Murchie, Scott L.
Robinson, Mark S.
Solomon, Sean C.
Denevi, Brett W.
Andre, Sarah L.
Head, James W.
TI Emplacement and tectonic deformation of smooth plains in the Caloris
basin, Mercury
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; MESSENGER; Caloris basin; tectonics; geologic history
ID WRINKLE RIDGES; MARE SERENITATIS; VOLCANISM; FLYBY; REFLECTANCE;
MESSENGER; ORIGIN; SLIP; MOON; TOPOGRAPHY
AB MESSENGER's first flyby of Mercury provided the first complete view of the Caloris basin and its interior smooth plains. Multispectral imaging shows that the interior plains are spectrally distinct from surrounding terrain, with a reflectance about 15-20% higher and a steeper spectral slope than the global average. The Caloris basin rim massifs and hummocky material, in contrast, have lower reflectance and a shallower spectral slope than the global average and extend around the entire basin. Isolated, relatively red patches along the margins of Caloris each surround irregularly shaped, scalloped-edged, rimless depressions that are interpreted to be volcanic vents, some with associated pyroclastic deposits. A nearly continuous annulus of smooth plains exterior to the basin displays spectral characteristics that contrast sharply with those of the basin-interior smooth plains. The exterior smooth plains are lower in reflectance and spectrally similar to the Caloris rim massifs and the hummocky materials. The rims and floors of larger impact craters in the interior plains expose low-reflectance material. There is widespread evidence of contractional and extensional tectonic deformation of the Caloris interior smooth plains. A set of linear radial graben, Pantheon Fossae, radiates outward from a zone near the basin center, and some of these graben extend to and intersect a set of generally basin-concentric graben distributed along the outer margin of the Caloris basin floor. The average areal extensional strain expressed by the mapped system of graben is similar to 0.08%. Wrinkle ridges also deform the interior smooth plains and predate both basin-radial and basin-concentric graben. The average areal contractional strain expressed by the mapped wrinkle ridges is similar to 0.07%. The density of wrinkle ridges on the western interior smooth plains is less than on the eastern interior plains, in contrast to the more even distribution of graben. A similar difference is seen between the density of wrinkle ridges on the western and eastern exterior smooth plains, with far fewer wrinkle ridges per unit area on the western annular plains. Superposition relations, spectral contrast, and the occurrence of volcanic vents and possible pyroclastic deposits all support a volcanic origin for the Caloris interior plains. Crater counts indicate that the Caloris exterior plains and hummocky material are younger than the Caloris rim and interior plains and are therefore also likely volcanic in origin. The contrast in spectral properties between the interior and exterior plains indicates a difference in the composition of the two expanses of volcanic material. Models for extensional tectonic deformation of the Caloris basin interior inferred from the distribution of graben viewed by Mariner 10 must be reevaluated to account for the discovery of Pantheon Fossae. Published by Elsevier B.V.
C1 [Watters, Thomas R.; Andre, Sarah L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Robinson, Mark S.; Denevi, Brett W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
EM watterst@si.edu
RI Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015
OI Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751
FU NASA [NASW-00002, NAS5-97271, NNX07AR60G]
FX We thank B. Ray Hawke and Walter S. Kiefer for helpful comments that
improved the manuscript. The MESSENGER mission is supported by the NASA
Discovery Program through contracts NASW-00002 to the Carnegie
Institution of Washington and NAS5-97271 to the Johns Hopkins University
Applied Physics Laboratory. This work was also supported by NASA grant
NNX07AR60G.
NR 57
TC 33
Z9 33
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 15
PY 2009
VL 285
IS 3-4
BP 309
EP 319
DI 10.1016/j.epsl.2009.03.040
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000009
ER
PT J
AU Freed, AM
Solomon, SC
Watters, TR
Phillips, RJ
Zuber, MT
AF Freed, Andrew M.
Solomon, Sean C.
Watters, Thomas R.
Phillips, Roger J.
Zuber, Maria T.
TI Could Pantheon Fossae be the result of the Apollodorus crater-forming
impact within the Caloris basin, Mercury?
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mercury; Caloris basin; Pantheon Fossae; Apollodorus crater
ID MESSENGER; VOLCANISM; FLYBY
AB The similar to 40-km-diameter Apollodorus impact crater lies near the center of Pantheon Fossae, a complex of radiating linear troughs itself at the approximate center of the 1500-km-diameter Caloris basin on Mercury. Here we use a series of finite element models to explore the idea that the Apollodorus crater-forming impact induced the formation of radially oriented graben by altering a pre-existing extensional stress state. Graben in the outer portions of the Caloris basin, which display predominantly circumferential orientations, have been taken as evidence that the basin interior was in a state of horizontal extensional stress as a result of uplift. If the Apollodorus crater formed at the time of such a stress state, impact-induced damage to basin fill material would have caused basin material to move radially outward, leading to a decrease in the radial extensional stress and an increase in the circumferential stress. If this change in differential stress was sufficient to induce failure, the predicted style of faulting would be radial graben extending outward from the exterior crater rim. The similar to 230-km radial extent of Pantheon Fossae implies, by this scenario, that the Apollodorus impact generated a large damage zone, extending to perhaps three crater radii (similar to 60 km) or more. The calculations also suggest, under this scenario, that the Caloris basin fill had greater strength than the surrounding crust and that the basin uplift and extensional stress field prior to the Apollodorus impact were close to azimuthally symmetric. The location of Pantheon Fossae very near the center of the Caloris basin appears to be coincidental; any crater similar in size to Apollodorus and located within similar to 300 km of the basin center could have produced a radiating set of graben by the mechanism explored here. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Freed, Andrew M.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
[Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Freed, AM (reprint author), Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
EM freed@purdue.edu
FU NASA [NASW-00002, NAS5-97271]
FX We thank William McKinnon and an anonymous reviewer for helpful comments
on an earlier draft. The MESSENGER mission is supported by the NASA
Discovery Program under contracts NASW-00002 to the Carnegie Institution
of Washington and NAS5-97271 to the Johns Hopkins University Applied
Physics Laboratory.
NR 19
TC 14
Z9 14
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 15
PY 2009
VL 285
IS 3-4
BP 320
EP 327
DI 10.1016/j.epsl.2009.02.038
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 504VN
UT WOS:000270646000010
ER
PT J
AU Farrell, WM
Plaut, JJ
Cummer, SA
Gurnett, DA
Picardi, G
Watters, TR
Safaeinili, A
AF Farrell, W. M.
Plaut, J. J.
Cummer, S. A.
Gurnett, D. A.
Picardi, G.
Watters, T. R.
Safaeinili, A.
TI Is the Martian water table hidden from radar view?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MARS; SUBSURFACE; IONOSPHERE; SOUNDINGS; DEPOSITS
AB Mars may possess a global sub-surface groundwater table as an integral part of its current hydrological system. However, the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) onboard the Mars Express (MEx) spacecraft has yet to make a definitive detection of such a body of liquid water. In this work, we quantify the conditions that would allow a detection of a deep aquifer and demonstrate that the lack of radar detection does not uniquely rule out the presence of such a body. Specifically, if the overlying crustal material has a conductivity above similar to 10(-5) S/m ( equivalent to a loss tanget of 0.008), a radar echo from an aquifer could be sufficiently attenuated by the intervening medium to prevent its detection by MARSIS. As such, the lack of direct detection by MARSIS-a "null result''-does not rule out the possibility of the water table's existence. Citation: Farrell, W. M., J. J. Plaut, S. A. Cummer, D. A. Gurnett, G. Picardi, T. R. Watters, and A. Safaeinili (2009), Is the Martian water table hidden from radar view?, Geophys. Res. Lett., 36, L15206, doi: 10.1029/2009GL038945.
C1 [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cummer, S. A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Picardi, G.] Univ Rome, Infocom Dept, I-00184 Rome, Italy.
[Plaut, J. J.; Safaeinili, A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Watters, T. R.] Smithsonian Inst, NASM, CEPS, Washington, DC 20560 USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM william.m.farrell@gsfc.nasa.gov
RI Cummer, Steven/A-6118-2008; Farrell, William/I-4865-2013
OI Cummer, Steven/0000-0002-0002-0613;
NR 20
TC 14
Z9 14
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 14
PY 2009
VL 36
AR L15206
DI 10.1029/2009GL038945
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 484EO
UT WOS:000269026600002
ER
PT J
AU Deacon, NR
Groot, PJ
Drew, JE
Greimel, R
Hambly, NC
Irwin, MJ
Aungwerojwit, A
Drake, J
Steeghs, D
AF Deacon, N. R.
Groot, P. J.
Drew, J. E.
Greimel, R.
Hambly, N. C.
Irwin, M. J.
Aungwerojwit, A.
Drake, J.
Steeghs, D.
TI The IPHAS-POSS-I proper motion survey of the Galactic plane
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; astrometry
ID H-ALPHA SURVEY; SKY SURVEY; STARS; CATALOG; DISCOVERY; NEBULA; YR(-1);
UKIDSS
AB We present a proper motion survey of the Galactic plane, using Isaac Newton Telescope (INT) Photometric H alpha Survey (IPHAS) data and Palomar Sky Survey (POSS)-I Schmidt plate data as a first epoch, that probes down to proper motions below 50 mas yr(-1). The IPHAS survey covers the northern plane (vertical bar b vertical bar < 5 degrees) with CCD photometry in the r, i and H alpha passbands. We examine roughly 1400 deg(2) of the IPHAS survey area and draw up a catalogue containing 103 058 objects with significant proper motions below 150 mas yr(-1) in the magnitude range 13.5 < r' < 19. Our survey sample contains large samples of white dwarfs and subdwarfs which can be identified using a reduced proper motion diagram. We also found several objects with IPHAS colours suggesting H alpha emission and significant proper motions. One is the known cataclysmic variable GD552; two are known DB white dwarfs and five others are found to be non-DA (DB and DC) white dwarfs, which were included in the H alpha emission line catalogue due to their lack of absorption in the H alpha narrow band.
C1 [Deacon, N. R.; Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Drew, J. E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Greimel, R.] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain.
[Greimel, R.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria.
[Hambly, N. C.] Univ Edinburgh, Royal Observ Edinburgh, Sch Phys, Inst Astron,SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Irwin, M. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Aungwerojwit, A.] Naresuan Univ, Fac Sci, Dept Phys, Phitsanulok 65000, Thailand.
[Aungwerojwit, A.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Drake, J.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Deacon, NR (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM ndeacon@astro.ru.nl
RI Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016;
OI Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X;
Drew, Janet/0000-0003-1192-7082
FU NOVA; NWO-VIDI [639.041.405]
FX This paper uses data from the supercosmos Sky Survey and from the IPHAS
of the northern Galactic plane carried out at the Isaac Newton Telescope
(INT). The INT is 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. All IPHAS data are processed by
the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in
Cambridge. NRD is funded by NOVA and PG by NWO-VIDI grant 639.041.405.
DS acknowledges a STFC Advanced Fellowship. This paper makes use of
sSlalib routines (see Wallace 1998). This research has made use of the
simbad data base, operated at CDS, Strasbourg, France. We thank the FAST
observers for their assistance with obtaining the followup spectroscopy
of IPHAS emitters. The 1.5-m Tillinghast telescope is located near Mt.
Hopkins in Arizona and operated on behalf of the Smithsonian
Astrophysical Observatory. The authors would like to thank Boris
Gaensicke, Christian Knigge, Quentin Parker and Stuart Sale for their
helpful comments.
NR 30
TC 7
Z9 7
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 11
PY 2009
VL 397
IS 3
BP 1685
EP 1694
DI 10.1111/j.1365-2966.2009.15077.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 476RB
UT WOS:000268459900044
ER
PT J
AU Laycock, S
Drake, JJ
AF Laycock, Silas
Drake, Jeremy J.
TI A FLARING X-RAY SOURCE WITH AN H alpha-BRIGHT COUNTERPART TOWARD THE
SMALL MAGELLANIC CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Magellanic Clouds; stars: coronae; stars: flare; X-rays: stars
ID EMISSION; BINARIES; EINSTEIN; SPECTRA; PLASMA; FIELDS; STARS
AB We report the discovery of a flaring X-ray source with an optical counterpart with H alpha emission and red-excess, in the direction of the Small Magellanic Cloud. A 100 ks X-ray observation with Chandra detected a flare lasting similar to 6 ks in the source CXO J005428.9-723107. The X-ray spectrum during the flare was consistent with a thermal plasma of temperature kT = 2.4 +/- 0.4 keV. In quiescence following the flare the spectrum was softer (kT similar to 0.4 keV). Timing analysis did not reveal any significant periodicities or quasi-periodic oscillations. Optical images taken with the Magellan-Baade 6.5 m telescope show a single star in the (0 ''.9) error circle. This star has apparent magnitude V = 19.17, exhibits enhanced H alpha emission (H alpha - r = -0.88 +/- 0.02), and has a large proper motion. Alternative explanations are explored, leading to identification as a relatively nearby (Galactic) coronally active binary star of the BY Draconis class.
C1 [Laycock, Silas] Gemini Observ, Hilo, HI 96720 USA.
[Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Laycock, S (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA.
EM silas@gemini.edu
FU Gemini Observatory; NASA [NAS8-39073]
FX This work was supported by the Gemini Observatory, which is operated by
the Association of Universities for Research in Astronomy, Inc., on
behalf of the International Gemini partnership of Argentina, Australia,
Brazil, Canada, Chile, the United Kingdom, and the United States of
America. J. J. D. was funded by NASA contract NAS8-39073 to the Chandra
X-ray Center during the course of this research. We thank Maureen van
den Berg for providing the Magellan images.
NR 28
TC 3
Z9 3
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 12
EP 17
DI 10.1088/0004-637X/701/1/12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800003
ER
PT J
AU Staniszewski, Z
Ade, PAR
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Halverson, NW
Holder, GP
Holzapfel, WL
Hrubes, JD
Joy, M
Keisler, R
Lanting, TM
Lee, AT
Leitch, EM
Loehr, A
Lueker, M
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Ngeow, CC
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Ruhl, JE
Schaffer, KK
Shaw, L
Shirokoff, E
Spieler, HG
Stalder, B
Stark, AA
Vanderlinde, K
Vieira, JD
Zahn, O
Zenteno, A
AF Staniszewski, Z.
Ade, P. A. R.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. -M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Joy, M.
Keisler, R.
Lanting, T. M.
Lee, A. T.
Leitch, E. M.
Loehr, A.
Lueker, M.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Ngeow, C. -C.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Ruhl, J. E.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spieler, H. G.
Stalder, B.
Stark, A. A.
Vanderlinde, K.
Vieira, J. D.
Zahn, O.
Zenteno, A.
TI GALAXY CLUSTERS DISCOVERED WITH A SUNYAEV-ZEL'DOVICH EFFECT SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; cosmology: observations; galaxies:
clusters: general
ID SOUTH-POLE TELESCOPE; SOURCE CATALOG; POWER SPECTRUM; CONSTRAINTS;
ENERGY; SCALE; MASS; ANISOTROPIES; COSMOLOGY; UNIVERSE
AB The South Pole Telescope (SPT) is conducting a Sunyaev-Zel'dovich (SZ) effect survey over large areas of the southern sky, searching for massive galaxy clusters to high redshift. In this preliminary study, we focus on a 40 deg(2) area targeted by the Blanco Cosmology Survey (BCS), which is centered roughly at right ascension 5(h)30(m), declination -53 degrees (J2000). Over two seasons of observations, this entire region has been mapped by the SPT at 95 GHz, 150 GHz, and 225 GHz. We report the four most significant SPT detections of SZ clusters in this field, three of which were previously unknown and, therefore, represent the first galaxy clusters discovered with an SZ survey. The SZ clusters are detected as decrements with greater than 5 sigma significance in the high-sensitivity 150 GHz SPT map. The SZ spectrum of these sources is confirmed by detections of decrements at the corresponding locations in the 95 GHz SPT map and nondetections at those locations in the 225 GHz SPT map. Multiband optical images from the BCS survey demonstrate significant concentrations of similarly colored galaxies at the positions of the SZ detections. Photometric redshift estimates from the BCS data indicate that two of the clusters lie at moderate redshift (z similar to 0.4) and two at high redshift (z greater than or similar to 0.8). One of the SZ detections was previously identified as a galaxy cluster in the optical as part of the Abell supplementary southern cluster catalog and in the X-ray using data from the ROSAT All-Sky Survey (RASS). Potential RASS counterparts (not previously identified as clusters) are also found for two of the new discoveries. These first four galaxy clusters are the most significant SZ detections from a subset of the ongoing SPT survey. As such, they serve as a demonstration that SZ surveys, and the SPT in particular, can be an effective means for finding galaxy clusters.
C1 [Staniszewski, Z.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Staniszewski, Z.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vanderlinde, K.; Vieira, J. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Cho, H. -M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Mehl, J.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Pryke, C.; Vanderlinde, K.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.; Vanderlinde, K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[de Haan, T.; Dobbs, M. A.; Holder, G. P.; Lanting, T. M.; Shaw, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Loehr, A.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mohr, J. J.; Ngeow, C. -C.; Zenteno, A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Mohr, J. J.; Ngeow, C. -C.; Zenteno, A.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Staniszewski, Z (reprint author), Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
EM tcrawfor@kicp.uchicago.edu
RI Holzapfel, William/I-4836-2015;
OI Aird, Kenneth/0000-0003-1441-9518; Reichardt,
Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996
NR 53
TC 153
Z9 153
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 32
EP 41
DI 10.1088/0004-637X/701/1/32
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800005
ER
PT J
AU Cranmer, SR
AF Cranmer, Steven R.
TI A PULSATIONAL MECHANISM FOR PRODUCING KEPLERIAN DISKS AROUND Be STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE circumstellar matter; stars: early-type; stars: emission-line, Be;
stars: oscillations; stars: rotation; waves
ID LINE-PROFILE VARIATIONS; DRIVEN STELLAR WINDS; B-TYPE STARS;
ANGULAR-MOMENTUM TRANSPORT; ACOUSTIC-WAVE PROPAGATION; INTERNAL
GRAVITY-WAVES; EPISODIC MASS-LOSS; FREQUENCY G-MODES; POINT-OF-VIEW;
SOLAR ATMOSPHERE
AB Classical Be stars are an enigmatic subclass of rapidly rotating hot stars characterized by dense equatorial disks of gas that have been inferred to orbit with Keplerian velocities. Although these disks seem to be ejected from the star and not accreted, there is substantial observational evidence to show that the stars rotate more slowly than required for centrifugally driven mass loss. This paper develops an idea (proposed originally by Hiroyasu Ando and colleagues) that nonradial stellar pulsations inject enough angular momentum into the upper atmosphere to spin up a Keplerian disk. The pulsations themselves are evanescent in the stellar photosphere, but they may be unstable to the generation of resonant oscillations at the acoustic cutoff frequency. A detailed theory of the conversion from pulsations to resonant waves does not yet exist for realistic hot-star atmospheres, so the current models depend on a parameterized approximation for the efficiency of wave excitation. Once resonant waves have been formed, however, they grow in amplitude with increasing height, steepen into shocks, and exert radial and azimuthal Reynolds stresses on the mean fluid. Using reasonable assumptions for the stellar parameters, these processes were found to naturally create the inner boundary conditions required for dense Keplerian disks, even when the underlying B-star photosphere is rotating as slowly as 60% of its critical rotation speed. Because there is evidence for long-term changes in Be-star pulsational properties, this model may also account for the long-term variability of Be stars, including transitions between normal, Be, and shell phases.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 170
TC 27
Z9 27
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 396
EP 413
DI 10.1088/0004-637X/701/1/396
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800033
ER
PT J
AU Ashby, MLN
Stern, D
Brodwin, M
Griffith, R
Eisenhardt, P
Kozlowski, S
Kochanek, CS
Bock, JJ
Borys, C
Brand, K
Brown, MJI
Cool, R
Cooray, A
Croft, S
Dey, A
Eisenstein, D
Gonzalez, AH
Gorjian, V
Grogin, NA
Ivison, RJ
Jacob, J
Jannuzi, BT
Mainzer, A
Moustakas, LA
Rottgering, HJA
Seymour, N
Smith, HA
Stanford, SA
Stauffer, JR
Sullivan, I
van Breugel, W
Willner, SP
Wright, EL
AF Ashby, M. L. N.
Stern, D.
Brodwin, M.
Griffith, R.
Eisenhardt, P.
Kozlowski, S.
Kochanek, C. S.
Bock, J. J.
Borys, C.
Brand, K.
Brown, M. J. I.
Cool, R.
Cooray, A.
Croft, S.
Dey, A.
Eisenstein, D.
Gonzalez, A. H.
Gorjian, V.
Grogin, N. A.
Ivison, R. J.
Jacob, J.
Jannuzi, B. T.
Mainzer, A.
Moustakas, L. A.
Rottgering, H. J. A.
Seymour, N.
Smith, H. A.
Stanford, S. A.
Stauffer, J. R.
Sullivan, I.
van Breugel, W.
Willner, S. P.
Wright, E. L.
TI THE SPITZER DEEP, WIDE-FIELD SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: galaxies; infrared: stars; surveys
ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; INFRARED ARRAY CAMERA; IRAC
SHALLOW SURVEY; GALAXY LUMINOSITY FUNCTIONS; SURVEY COMMISSIONING DATA;
RADIO-LOUD AGN; X-RAY SURVEY; SPACE-TELESCOPE; BOOTES-FIELD
AB The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg(2) in the Bootes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit-for the first time-the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z similar to 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z similar to 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 x 10(5) distinct sources detected to the average 5 sigma, 4 ''-diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 mu m, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, > 50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and > 80% of on-axis XBootes sources are detected out to 8.0 mu m. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class.
C1 [Ashby, M. L. N.; Brodwin, M.; Smith, H. A.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, D.; Griffith, R.; Eisenhardt, P.; Gorjian, V.; Jacob, J.; Mainzer, A.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kozlowski, S.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Bock, J. J.; Borys, C.] CALTECH, Pasadena, CA 91125 USA.
[Brand, K.; Grogin, N. A.; Sullivan, I.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Cool, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Cooray, A.] Univ Calif Irvine, Irvine, CA 92697 USA.
[Croft, S.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Eisenstein, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Leiden Univ, Leiden Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Seymour, N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA.
[Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[van Breugel, W.] Univ Calif, Merced, CA 95344 USA.
[Wright, E. L.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mashby@cfa.harvard.edu
RI Kozlowski, Szymon/G-4799-2013; Brown, Michael/B-1181-2015; Ivison,
R./G-4450-2011;
OI Kozlowski, Szymon/0000-0003-4084-880X; Brown,
Michael/0000-0002-1207-9137; Ivison, R./0000-0001-5118-1313; Seymour,
Nicholas/0000-0003-3506-5536; Moustakas, Leonidas/0000-0003-3030-2360;
Croft, Steve/0000-0003-4823-129X
FU National Aeronautics and Space Administration (NASA); NASA [1314516,
NCC5-626]; NASA's Earth Science Technology Office; California Institute
of Technology; W.M. Keck Foundation
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under contract with the National
Aeronautics and Space Administration (NASA). Support for this work was
provided by NASA through award number 1314516 issued by JPL/Caltech.
This research made use of Montage, funded by the NASA's Earth Science
Technology Office, Computation Technologies Project, under Cooperative
Agreement Number NCC5-626 between NASA and the California Institute of
Technology. Montage is maintained by the NASA/IPAC Infrared Science
Archive. IRAF is distributed by the 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. Support for M. B. was provided by the W.M.
Keck Foundation. The authors thank Andy Gould, whose suggestions
improved the manuscript.
NR 79
TC 127
Z9 127
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 428
EP 453
DI 10.1088/0004-637X/701/1/428
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800036
ER
PT J
AU Voss, R
Gilfanov, M
Sivakoff, GR
Kraft, RP
Jordan, A
Raychaudhury, S
Birkinshaw, M
Brassington, NJ
Croston, JH
Evans, DA
Forman, WR
Hardcastle, MJ
Harris, WE
Jones, C
Juett, AM
Murray, SS
Sarazin, CL
Woodley, KA
Worrall, DM
AF Voss, Rasmus
Gilfanov, Marat
Sivakoff, Gregory R.
Kraft, Ralph P.
Jordan, Andres
Raychaudhury, Somak
Birkinshaw, Mark
Brassington, Nicola J.
Croston, Judith H.
Evans, Daniel A.
Forman, William R.
Hardcastle, Martin J.
Harris, William E.
Jones, Christine
Juett, Adrienne M.
Murray, Stephen S.
Sarazin, Craig L.
Woodley, Kristin A.
Worrall, Diana M.
TI LUMINOSITY FUNCTIONS OF LMXBs IN CENTAURUS A: GLOBULAR CLUSTERS VERSUS
THE FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (Centaurus A); X-rays: binaries; X-rays: galaxies
ID X-RAY BINARIES; POINT-SOURCE POPULATION; HOT INTERSTELLAR-MEDIUM;
XMM-NEWTON OBSERVATIONS; EARLY-TYPE GALAXIES; CHANDRA OBSERVATIONS;
ELLIPTIC GALAXIES; PARTICLE-ACCELERATION; ULTRACOMPACT BINARIES;
RADIO-LOBE
AB We study the X-ray luminosity function (XLF) of low-mass X-ray binaries (LMXB) in the nearby early-type galaxy Centaurus A, concentrating primarily on two aspects of binary populations: the XLF behavior at the low-luminosity limit and the comparison between globular cluster and field sources. The 800 ksec exposure of the deep Chandra VLP program allows us to reach a limiting luminosity of similar to 8 x 10(35) erg s(-1), about similar to 2-3 times deeper than previous investigations. We confirm the presence of the low-luminosity break of the overall LMXB XLF at log(L(X)) approximate to 37.2-37.6, below which the luminosity distribution follows a dN/d(lnL) similar to const law. Separating globular cluster and field sources, we find a statistically significant difference between the two luminosity distributions with a relative underabundance of faint sources in the globular cluster population. This demonstrates that the samples are drawn from distinct parent populations and may disprove the hypothesis that the entire LMXB population in early-type galaxies is created dynamically in globular clusters. As a plausible explanation for this difference in the XLFs, we suggest an enhanced fraction of helium-accreting systems in globular clusters, which are created in collisions between red giants and neutron stars. Due to the four times higher ionization temperature of He, such systems are subject to accretion disk instabilities at approximate to 20 times higher mass accretion rate and, therefore, are not observed as persistent sources at low luminosities.
C1 [Voss, Rasmus] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Voss, Rasmus] Tech Univ Munich, D-85748 Garching, Germany.
[Gilfanov, Marat] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Gilfanov, Marat] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia.
[Sivakoff, Gregory R.; Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Sivakoff, Gregory R.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA.
[Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England.
[Croston, Judith H.; Hardcastle, Martin J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Evans, Daniel A.] MIT, Kavli Inst, Cambridge, MA 02139 USA.
[Forman, William R.; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Harris, William E.; Woodley, Kristin A.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
RP Voss, R (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM rvoss@mpe.mpg.de; grs8g@virginia.edu
RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011;
OI Hardcastle, Martin/0000-0003-4223-1117; Sivakoff,
Gregory/0000-0001-6682-916X; Jordan, Andres/0000-0002-5389-3944
FU NASA [GO7-8105X, NAS8-03060]; Royal Society; [HST-GO-10597.03-A];
[HST-GO-10582.02-A]; [HST-GO-10835.01-A]; [GO8-9085X]
FX This research has made use of data obtained from the Chandra Data
Archive and software provided by the Chandra X-ray Center (CXC) in the
application package CIAO. This work was supported by the NASA grants
GO7-8105X and NAS8-03060. R. V. acknowledges the support by the DFG
cluster of excellence "Origin and Structure of the Universe"
(http://www.universe-cluster.de). C. L. S. and G. R. S. were supported
in part by Hubble grants HST-GO-10597.03-A, HST-GO-10582.02-A, and
HST-GO-10835.01-A, and Chandra grant GO8-9085X. M. S. H. thanks the
Royal Society for support. The authors would also like to thank the
anonymous referee for constructive criticism of the original manuscript
that helped to improve the paper.
NR 60
TC 26
Z9 26
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 471
EP 480
DI 10.1088/0004-637X/701/1/471
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800039
ER
PT J
AU Machalek, P
McCullough, PR
Burrows, A
Burke, CJ
Hora, JL
Johns-Krull, CM
AF Machalek, Pavel
McCullough, Peter R.
Burrows, Adam
Burke, Christopher J.
Hora, Joseph L.
Johns-Krull, Christopher M.
TI DETECTION OF THERMAL EMISSION OF XO-2b: EVIDENCE FOR A WEAK TEMPERATURE
INVERSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; infrared: stars; planetary systems; stars:
individual (XO-2)
ID EXTRASOLAR GIANT PLANETS; EXOPLANET HD 189733B; LIGHT CURVES; SPECTRUM;
ATMOSPHERES; 209458B; SEARCH; HOT
AB We estimate flux ratios of the extrasolar planet XO-2b to its host star XO-2 at 3.6, 4.5, 5.8, and 8.0 mu m with Infrared Array Camera on the Spitzer Space Telescope to be 0.00081 +/- 0.00017, 0.00098 +/- 0.00020, 0.00167 +/- 0.00036, and 0.00133 +/- 0.00049, respectively. The fluxes provide tentative evidence for a weak temperature inversion in the upper atmosphere, the precise nature of which would need to be confirmed by longer wavelength observations. XO-2b substellar flux of 0.76 x 10(9) erg cm(-2) s(-1) lies in the predicted transition region between atmospheres with and without upper atmospheric temperature inversion.
C1 [Machalek, Pavel] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Machalek, Pavel; McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Burke, Christopher J.; Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
RP Machalek, P (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM pavel@jhu.edu
OI Hora, Joseph/0000-0002-5599-4650
FU Spitzer Science Center [C4030]; NASA [NNX07AG80G]; JPL/Spitzer [1328092,
1348668, 1312647]; National Aeronautics and Space Administration;
National Science Foundation
FX The authors thank H. Knutson and N. Iro for helpful discussions. The
authors also acknowledge the use of publicly available routines by Eric
Agol and the Levenberg-Marquardt least-squares minimization routine
MPFITFUN by Craig Markwardt. P. M. and P. R. M. were supported by the
Spitzer Science Center grant C4030 to the Space Telescope Science
Institute. A. B. was supported in part by NASA grant NNX07AG80G. We also
acknowledge support through JPL/Spitzer Agreements 1328092, 1348668, and
1312647. This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. This
publication also makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation.
NR 31
TC 41
Z9 41
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 514
EP 520
DI 10.1088/0004-637X/701/1/514
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800044
ER
PT J
AU Chan, CK
Liu, SM
Fryer, CL
Psaltis, D
Ozel, F
Rockefeller, G
Melia, F
AF Chan, Chi-Kwan
Liu, Siming
Fryer, Christopher L.
Psaltis, Dimitrios
Oezel, Feryal
Rockefeller, Gabriel
Melia, Fulvio
TI MHD SIMULATIONS OF ACCRETION ONTO Sgr A*: QUIESCENT FLUCTUATIONS,
OUTBURSTS, AND QUASIPERIODICITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; Galaxy: center;
instabilities; MHD; relativity
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; SUPERMASSIVE BLACK-HOLE;
X-RAY FLARE; ROSSBY-WAVE INSTABILITY; SAGITTARIUS-A; GALACTIC-CENTER;
SPECTRAL METHODS; ELECTRON ACCELERATION; HYDRODYNAMIC DISKS;
ANGULAR-MOMENTUM
AB High-resolution observations of Sgr A* have revealed a wide variety of phenomena, ranging from intense rapid flares to quasi-periodic oscillations (QPOs), making this object an ideal system to study the properties of low luminosity accreting black holes. In this paper, we use a pseudospectral algorithm to construct and evolve a three-dimensional magnetohydrodynamic (MHD) model of the accretion disk in Sgr A*. Assuming a hybrid thermal nonthermal emission scheme and calibrating the parameters by observations, we show that the MHD turbulence in the environment of Sgr A* can by itself only produce factor two fluctuations in luminosity. These fluctuations cannot explain the magnitude of flares observed in this system. However, we also demonstrate that external forcing of the accretion disk, which may be generated by the "clumpy material" raining down onto the disk from the large-scale flow, do produce outbursts qualitatively similar to those observed by XMM-Newton in X-rays and by ground- based facilities in the near infrared. Strong, but short-term QPOs emerge naturally in the simulated light curves. We attribute these to nonaxisymmetric density perturbations that emerge as the disk evolves back toward its quiescent state.
C1 [Chan, Chi-Kwan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Chan, Chi-Kwan; Fryer, Christopher L.; Psaltis, Dimitrios; Oezel, Feryal; Melia, Fulvio] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Liu, Siming] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Fryer, Christopher L.; Rockefeller, Gabriel] Los Alamos Natl Lab, Computat Comp Sci Div, Los Alamos, NM 87545 USA.
[Psaltis, Dimitrios; Oezel, Feryal; Melia, Fulvio] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
RI Rockefeller, Gabriel/G-2920-2010; liu, siming/B-5389-2011
OI Rockefeller, Gabriel/0000-0002-9029-5097;
FU U.S. Department of Energy at Los Alamos National Laboratory
[DE-AC52-06NA25396]; NSF [AST-0402502]; NASA ATP [NAG5-13374]
FX This work was carried out under the auspices of the National Nuclear
Security Administration of the U.S. Department of Energy at Los Alamos
National Laboratory under Contract No. DE-AC52-06NA25396. At the
University of Arizona, this research was supported by NSF grant
AST-0402502 and NASA ATP grant NAG5-13374. F. M. is grateful to the
University of Melbourne for its support (through a Sir Thomas Lyle
Fellowship and a Miegunyah Fellowship). The simulations were carried out
on the Space Simulator at Los Alamos National Laboratory and on a
Beowulf cluster in the Physics Department at the University of Arizona.
NR 74
TC 32
Z9 32
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 521
EP 534
DI 10.1088/0004-637X/701/1/521
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800045
ER
PT J
AU Wu, YL
Charmandaris, V
Huang, JS
Spinoglio, L
Tommasin, S
AF Wu, Yanling
Charmandaris, Vassilis
Huang, Jiasheng
Spinoglio, Luigi
Tommasin, Silvia
TI SPITZER/IRS 5-35 mu m LOW-RESOLUTION SPECTROSCOPY OF THE 12 mu m SEYFERT
SAMPLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: starburst; infrared:
galaxies; techniques: spectroscopic
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; POLYCYCLIC
AROMATIC-HYDROCARBON; STAR-FORMATION RATE; X-RAY LUMINOSITY;
SPACE-TELESCOPE; MIDINFRARED SPECTRA; ENERGY-DISTRIBUTIONS; SILICATE
EMISSION; INTERSTELLAR DUST
AB We present low-resolution 5.5-35 mu m spectra for 103 galaxies from the 12 mu m Seyfert sample, a complete unbiased 12 mu m flux limited sample of local Seyfert galaxies selected from the IRAS Faint Source Catalog, obtained with the Infrared Spectrograph (IRS) on-board Spitzer Space Telescope. For 70 of the sources observed in the IRS mapping mode, uniformly extracted nuclear spectra are presented for the first time. We performed an analysis of the continuum emission, the strength of the polycyclic aromatic hydrocarbon (PAH) and astronomical silicate features of the sources. We find that on average, the 15-30 mu m slope of the continuum is = -0.85 +/- 0.61 for Seyfert 1s and -1.53 +/- 0.84 for Seyfert 2s, and there is substantial scatter in each type. Moreover, nearly 32% of the Seyfert 1s, and 9% of the Seyfert 2s, display a peak in the mid-infrared spectrum at 20 mu m, which is attributed to an additional hot dust component. The PAH equivalent width decreases with increasing dust temperature, as indicated by the global infrared color of the host galaxies. However, no statistical difference in PAH equivalent width is detected between the two Seyfert types, 1 and 2, of the same bolometric luminosity. The silicate features at 9.7 and 18 mu m in Seyfert 1 galaxies are rather weak, while Seyfert 2s are more likely to display strong silicate absorption. Those Seyfert 2s with the highest silicate absorption also have high infrared luminosity and high absorption (hydrogen column density N(H) > 10(23) cm(-2)) as measured from the X-rays. Finally, we propose a new method to estimate the active galactic nucleus contribution to the integrated 12 mu m galaxy emission, by subtracting the "star formation" component in the Seyfert galaxies, making use of the tight correlation between PAH 11.2 mu m luminosity and 12 mu m luminosity for star-forming galaxies.
C1 [Wu, Yanling] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Charmandaris, Vassilis] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Charmandaris, Vassilis] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece.
[Charmandaris, Vassilis] Observ Paris, Chercheur Assoc, F-75014 Paris, France.
[Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spinoglio, Luigi; Tommasin, Silvia] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Tommasin, Silvia] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
RP Wu, YL (reprint author), CALTECH, Ctr Infrared Proc & Anal, 1200 E Calif Blvd,MC 314-6, Pasadena, CA 91125 USA.
EM yanling@ipac.caltech.edu; vassilis@physics.uoc.gr;
jhuang@cfa.harvard.edu; luigi.spinoglio@ifsi-roma.inaf.it;
Silvia.Tommasin@ifsi-roma.inaf.it
RI Charmandaris, Vassilis/A-7196-2008; Wu, Yanling/A-1261-2010
OI Charmandaris, Vassilis/0000-0002-2688-1956;
FU EU ToK [39965]; Italian Space Agency (ASI)
FX V. C. acknowledges partial support from the EU ToK grant 39965. L. S.
and S. T. acknowledge support from the Italian Space Agency (ASI).
NR 86
TC 64
Z9 64
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 658
EP 676
DI 10.1088/0004-637X/701/1/658
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800056
ER
PT J
AU Fernandez, JM
Latham, DW
Torres, G
Everett, ME
Mandushev, G
Charbonneau, D
O'Donovan, FT
Alonso, R
Esquerdo, GA
Hergenrother, CW
Stefanik, RP
AF Fernandez, Jose M.
Latham, David W.
Torres, Guillermo
Everett, Mark E.
Mandushev, Georgi
Charbonneau, David
O'Donovan, Francis T.
Alonso, Roi
Esquerdo, Gilbert A.
Hergenrother, Carl W.
Stefanik, Robert P.
TI MASS AND RADIUS DETERMINATIONS FOR FIVE TRANSITING M-DWARF STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; binaries: spectroscopic; stars: fundamental
parameters; stars: low-mass, brown dwarfs; stars: rotation
ID HYDROGEN-BURNING LIMIT; DOPPLER FOLLOW-UP; ECLIPSING BINARY;
EVOLUTIONARY MODELS; SPECTROSCOPIC BINARIES; ABSOLUTE DIMENSIONS;
EXTRASOLAR PLANETS; KEPLER MISSION; Y-2 ISOCHRONES; LIGHT-CURVE
AB We have derived masses and radii for both components in five short-period single-lined eclipsing binary stars discovered by the TrES wide-angle photometric survey for transiting planets. All these systems consist of a visible F-star primary and an unseen M-star secondary (M(A) >= 0.8 M(circle dot), M(B) <= 0.45 M(circle dot)). The spectroscopic orbital solution combined with a high-precision transit light curve for each system gives sufficient information to calculate the density of the primary star and the surface gravity of the secondary. The masses of the primary stars were obtained using stellar evolution models, which requires accurate determinations of metallicities and effective temperatures. In our case, the uncertainty in the metallicity of the primary stars is the most important limiting factor in order to obtain accurate results for the masses and radii of the unseen M-dwarf secondaries. The solutions were compared with results obtained by calculating the radius of the primary stars under the assumption of rotational synchronization with the orbital period and alignment between their spin axis and the axis of the orbit, using the observed broadening of the spectral lines as an indicator of stellar rotation. Four systems show an acceptable match between the two sets of results when their metallicity is allowed to vary around solar values (-0.5 <= [Fe/H] <= +0.5), but one system shows a clear mismatch between the two solutions, which may indicate the absence of synchronization or a misalignment between the rotational and orbital axis. When compared to low-mass stellar evolution models, the derived masses and radii of the unseen M dwarfs are inconsistent (three only marginally) with the predicted values, with all of the radii being larger than expected for their masses. These results confirm the discrepancy shown in a previous work between the predicted and observed radii on low-mass binary stars. This work also shows that reliance on the assumption of synchronization to derive the mass and radius of stars in eclipsing single-lined F+M binaries is a useful tool, but may not always be warranted and should be carefully tested against stellar evolution models.
C1 [Fernandez, Jose M.; Latham, David W.; Torres, Guillermo; Charbonneau, David; Esquerdo, Gilbert A.; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fernandez, Jose M.] Pontificia Univ Catolica, Dept Astron, Santiago 22, Chile.
[Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA.
[Alonso, Roi] Technople Marseille Etoile, UMR 6110, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Hergenrother, Carl W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85719 USA.
RP Fernandez, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jfernand@cfa.harvard.edu
RI Alonso, Roi/D-8799-2014; O'Donovan, Francis/I-2423-2014;
OI Alonso, Roi/0000-0001-8462-8126; O'Donovan, Francis/0000-0002-4858-6106;
Charbonneau, David/0000-0002-9003-484X
FU NASA Cooperative Agreement [NCC2-1390]; NSF [AST-0708229]
FX This research was supported in part by the Kepler Mission under NASA
Cooperative Agreement NCC2-1390. G. T. acknowledges partial support from
NSF grant AST-0708229.
NR 45
TC 27
Z9 28
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2009
VL 701
IS 1
BP 764
EP 775
DI 10.1088/0004-637X/701/1/764
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 475ES
UT WOS:000268341800064
ER
PT J
AU Bovino, S
Zhang, P
Kharchenko, V
Dalgarno, A
AF Bovino, S.
Zhang, P.
Kharchenko, V.
Dalgarno, A.
TI Trapping hydrogen atoms from a neon-gas matrix: A theoretical simulation
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
DE ab initio calculations; atom-atom collisions; atomic forces; Boltzmann
equation; Bose-Einstein condensation; coupled cluster calculations;
hydrogen neutral atoms; neon
ID FAST NITROGEN-ATOMS; WAVE-FUNCTIONS; AB-INITIO; HYDRIDES;
THERMALIZATION; COEFFICIENTS; ENERGIES
AB Hydrogen is of critical importance in atomic and molecular physics and the development of a simple and efficient technique for trapping cold and ultracold hydrogen atoms would be a significant advance. In this study we simulate a recently proposed trap-loading mechanism for trapping hydrogen atoms released from a neon matrix. Accurate ab initio quantum calculations are reported of the neon-hydrogen interaction potential and the energy- and angular-dependent elastic scattering cross sections that control the energy transfer of initially cold atoms are obtained. They are then used to construct the Boltzmann kinetic equation, describing the energy relaxation process. Numerical solutions of the Boltzmann equation predict the time evolution of the hydrogen energy distribution function. Based on the simulations we discuss the prospects of the technique.
C1 [Bovino, S.; Zhang, P.; Kharchenko, V.; Dalgarno, A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
RP Dalgarno, A (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
EM pezhang@cfa.harvard.edu; adalgarno@cfa.harvard.edu
FU Office of Basic Energy Science; Office of Science; U.S. Department of
Energy; NASA [NNX07AR03]
FX The research of A. D. and P. Z. was supported by the Chemical Science,
Geoscience and Bioscience Division of the Office of Basic Energy
Science, Office of Science, U.S. Department of Energy and of V. K. by
NASA Grant No. NNX07AR03G. S. B. thanks ITAMP and the
Harvard-Smithsonian Center for Astrophysics for his participation in
their predoctoral program. We are grateful to Professor Claudio Cesar
and Dr. Paolo Crivelli for sharing the details of the proposed
experiment. The computational resources were provided by the National
Center for Atmospheric Research (NCAR).
NR 29
TC 10
Z9 10
U1 0
U2 8
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD AUG 7
PY 2009
VL 131
IS 5
AR 054302
DI 10.1063/1.3180822
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 481KT
UT WOS:000268809800013
PM 19673557
ER
PT J
AU Zachos, LG
AF Zachos, Louis G.
TI A new computational growth model for sea urchin skeletons
SO JOURNAL OF THEORETICAL BIOLOGY
LA English
DT Article
DE Echinoid; Theoretical morphology; Voronoi; Delaunay; Simulation
ID ECHINOIDS ECHINODERMATA; CORONAL SKELETON; MORPHOLOGY; CALCIFICATION;
REGENERATION; SPHERE
AB A newcomputational model has been developed to simulate growth of regular sea urchin skeletons. The model incorporates the processes of plate addition and individual plate growth into a composite model of whole-body (somatic) growth. A simple developmental model based on hypothetical morphogens underlies the assumptions used to define the simulated growth processes. The data model is based on a Delaunay triangulation of plate growth center points, using the dual Voronoi polygons to define plate topologies. A spherical frame of reference is used for growth calculations, with affine deformation of the sphere (based on a Young-Laplace membrane model) to result in an urchin-like three-dimensional form. The model verifies that the patterns of coronal plates in general meet the criteria of Voronoi polygonalization, that a morphogen/threshold inhibition model for plate addition results in the alternating plate addition pattern characteristic of sea urchins, and that application of the Bertalanffy growth model to individual plates results in simulated somatic growth that approximates that seen in living urchins. The model suggests avenues of research that could explain some of the distinctions between modern sea urchins and the much more disparate groups of forms that characterized the Paleozoic Era. (C) 2009 Elsevier Ltd. All rights reserved.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol MRC 121, Washington, DC 20013 USA.
RP Zachos, LG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol MRC 121, POB 37012, Washington, DC 20013 USA.
EM lg_zachos@alumni.utexas.net
OI Zachos, Louis/0000-0001-7246-5008
FU Geology Foundation of the Jackson School of Geosciences at the
University of Texas at Austin; Smithsonian Institution
FX The author is grateful to Jim Sprinkle, Chris Bell, Ann Molineux, Rich
Mooi, and Tim Rowe who served on his dissertation committee and for the
many hours they spent in helping to improve the results of this study.
Olaf Ellers made many helpful comments on an early version of the model,
Jacob Dafni graciously sent the author much of the raw data regarding
his studies of sea urchin growth, and David Raup helped to improve the
manuscript with his comments. This work was supported by the Geology
Foundation of the Jackson School of Geosciences at the University of
Texas at Austin, and by the Smithsonian Institution Fellowship Program.
NR 49
TC 11
Z9 11
U1 1
U2 7
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-5193
J9 J THEOR BIOL
JI J. Theor. Biol.
PD AUG 7
PY 2009
VL 259
IS 3
BP 646
EP 657
DI 10.1016/j.jtbi.2009.04.007
PG 12
WC Biology; Mathematical & Computational Biology
SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational
Biology
GA 559CM
UT WOS:000274798000026
PM 19376133
ER
PT J
AU Dechmann, DKN
Heucke, SL
Giuggioli, L
Safi, K
Voigt, CC
Wikelski, M
AF Dechmann, Dina K. N.
Heucke, Silke L.
Giuggioli, Luca
Safi, Kamran
Voigt, Christian C.
Wikelski, Martin
TI Experimental evidence for group hunting via eavesdropping in
echolocating bats
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE information transfer; network; Noctilio albiventris; sociality
ID INFORMATION-TRANSFER; LOCAL ENHANCEMENT; EPTESICUS-FUSCUS; FORAGING
SUCCESS; SOCIAL CALLS; EVOLUTION; LOCATION; VULTURES; NOCTILIO; COLONIES
AB Group foraging has been suggested as an important factor for the evolution of sociality. However, visual cues are predominantly used to gain information about group members' foraging success in diurnally foraging animals such as birds, where group foraging has been studied most intensively. By contrast, nocturnal animals, such as bats, would have to rely on other cues or signals to coordinate foraging. We investigated the role of echolocation calls as inadvertently produced cues for social foraging in the insectivorous bat Noctilio albiventris. Females of this species live in small groups, forage over water bodies for swarming insects and have an extremely short daily activity period. We predicted and confirmed that (i) free-ranging bats are attracted by playbacks of echolocation calls produced during prey capture, and that (ii) bats of the same social unit forage together to benefit from passive information transfer via the change in group members' echolocation calls upon finding prey. Network analysis of high-resolution automated radio telemetry confirmed that group members flew within the predicted maximum hearing distance 94+/-6 per cent of the time. Thus, echolocation calls also serve as intraspecific communication cues. Sociality appears to allow for more effective group foraging strategies via eavesdropping on acoustical cues of group members in nocturnal mammals.
C1 [Dechmann, Dina K. N.; Wikelski, Martin] Univ Konstanz, Dept Biol, D-78457 Constance, Germany.
[Dechmann, Dina K. N.; Heucke, Silke L.; Voigt, Christian C.] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany.
[Dechmann, Dina K. N.; Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Heucke, Silke L.] Univ Vienna, A-1090 Vienna, Austria.
[Giuggioli, Luca] Univ Bristol, Dept Engn Math, Bristol Ctr Complex Sci, Bristol BS8 1TR, Avon, England.
[Giuggioli, Luca] Univ Bristol, Sch Biol Sci, Bristol BS8 1TR, Avon, England.
[Giuggioli, Luca] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
[Safi, Kamran] Zool Soc London, Inst Zool, London NW1 4RY, England.
[Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany.
RP Dechmann, DKN (reprint author), Univ Konstanz, Dept Biol, D-78457 Constance, Germany.
EM ddechmann@orn.mpg.de
RI Dechmann, Dina/A-1827-2010; Safi, Kamran/B-2079-2008; Giuggioli,
Luca/J-2881-2012
OI Safi, Kamran/0000-0002-8418-6759;
FU Max Planck Institute for Ornithology, Radolfzell; German Science
Foundation [VO 890/11-1]; NSF [DEB-0083566]; DARPA [HR0011-05-1-0057]
FX For help with fieldwork, we want to thank Nicolas Ory, Daniel Obando
(and ART-S) as well as Edgar Perez, general manager of the Gamboa
Rainforest Resort. Thanks to Bjorn Siemers for letting us to use his
playback equipment. Patrick Kelley, Corey Tarwater and two referees
provided valuable comments to the manuscript. Funding was received from:
Max Planck Institute for Ornithology, Radolfzell; German Science
Foundation, grant VO 890/11-1 to C. C. V. and D. K. N. D.; NSF grant
DEB-0083566 and DARPA grant HR0011-05-1-0057 funded L. G.
NR 45
TC 66
Z9 67
U1 7
U2 60
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P R SOC B
JI Proc. R. Soc. B-Biol. Sci.
PD AUG 7
PY 2009
VL 276
IS 1668
BP 2721
EP 2728
DI 10.1098/rspb.2009.0473
PG 8
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 462RP
UT WOS:000267373700005
PM 19419986
ER
PT J
AU Raymond, JC
AF Raymond, John C.
TI Cosmic-Ray Acceleration in Supernova Remnants
SO SCIENCE
LA English
DT Editorial Material
ID EMISSION; SHOCKS; WAVE
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM raymond@cfa.harvard.edu
NR 11
TC 2
Z9 2
U1 0
U2 0
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 7
PY 2009
VL 325
IS 5941
BP 683
EP 684
DI 10.1126/science.1177743
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 480HF
UT WOS:000268723700024
PM 19661406
ER
PT J
AU Borucki, WJ
Koch, D
Jenkins, J
Sasselov, D
Gilliland, R
Batalha, N
Latham, DW
Caldwell, D
Basri, G
Brown, T
Christensen-Dalsgaard, J
Cochran, WD
DeVore, E
Dunham, E
Dupree, AK
Gautier, T
Geary, J
Gould, A
Howell, S
Kjeldsen, H
Lissauer, J
Marcy, G
Meibom, S
Morrison, D
Tarter, J
AF Borucki, W. J.
Koch, D.
Jenkins, J.
Sasselov, D.
Gilliland, R.
Batalha, N.
Latham, D. W.
Caldwell, D.
Basri, G.
Brown, T.
Christensen-Dalsgaard, J.
Cochran, W. D.
DeVore, E.
Dunham, E.
Dupree, A. K.
Gautier, T.
Geary, J.
Gould, A.
Howell, S.
Kjeldsen, H.
Lissauer, J.
Marcy, G.
Meibom, S.
Morrison, D.
Tarter, J.
TI Kepler's Optical Phase Curve of the Exoplanet HAT-P-7b
SO SCIENCE
LA English
DT Article
ID HOT JUPITERS
C1 [Borucki, W. J.; Koch, D.; Lissauer, J.; Morrison, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jenkins, J.; Caldwell, D.; DeVore, E.; Tarter, J.] SETI Inst, Mountain View, CA 94043 USA.
[Sasselov, D.; Latham, D. W.; Dupree, A. K.; Geary, J.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gilliland, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Batalha, N.] San Jose State Univ, San Jose, CA 95192 USA.
[Basri, G.; Marcy, G.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Brown, T.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, DK-8000 Aarhus, Denmark.
[Cochran, W. D.] Univ Texas Austin, Austin, TX 78712 USA.
[Dunham, E.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gould, A.] Lawrence Hall Sci, Berkeley, CA 94720 USA.
[Howell, S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM william.j.borucki@nasa.gov
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
FU NASA; Ball Aerospace; NASA Discovery program
FX We acknowledge the contributions of hundreds of individuals across NASA,
Ball Aerospace, and the scientific community who made this mission
possible. Funding was provided by the NASA Discovery program.
NR 5
TC 132
Z9 132
U1 0
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 7
PY 2009
VL 325
IS 5941
BP 709
EP 709
DI 10.1126/science.1178312
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 480HF
UT WOS:000268723700038
PM 19661420
ER
PT J
AU Roy, K
Hunt, G
Jablonski, D
AF Roy, Kaustuv
Hunt, Gene
Jablonski, David
TI Phylogenetic Conservatism of Extinctions in Marine Bivalves
SO SCIENCE
LA English
DT Article
ID FOSSIL RECORD; TAXONOMIC SELECTIVITY; MOLECULAR PHYLOGENIES; GEOGRAPHIC
RANGE; MASS EXTINCTIONS; DIVERSITY; HISTORY; PATTERNS; RATES;
MACROEVOLUTION
AB Evolutionary histories of species and lineages can influence their vulnerabilities to extinction, but the importance of this effect remains poorly explored for extinctions in the geologic past. When analyzed using a standardized taxonomy within a phylogenetic framework, extinction rates of marine bivalves estimated from the fossil record for the last similar to 200 million years show conservatism at multiple levels of evolutionary divergence, both within individual families and among related families. The strength of such phylogenetic clustering varies over time and is influenced by earlier extinction history, especially by the demise of volatile taxa in the end-Cretaceous mass extinction. Analyses of the evolutionary roles of ancient extinctions and predictive models of vulnerability of taxa to future natural and anthropogenic stressors should take phylogenetic relationships and extinction history into account.
C1 [Roy, Kaustuv] Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA.
[Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Jablonski, David] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
RP Roy, K (reprint author), Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA.
EM kroy@ucsd.edu
RI Hunt, Gene/B-3783-2010
OI Hunt, Gene/0000-0001-6430-5020
FU NASA
FX This work was supported by a grant from NASA.
NR 40
TC 39
Z9 39
U1 2
U2 32
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD AUG 7
PY 2009
VL 325
IS 5941
BP 733
EP 737
DI 10.1126/science.1173073
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 480HF
UT WOS:000268723700045
PM 19661426
ER
PT J
AU Butt, Y
AF Butt, Yousaf
TI Beyond the myth of the supernova-remnant origin of cosmic rays
SO NATURE
LA English
DT Article
ID MOLECULAR CLOUDS; OB ASSOCIATIONS; GALACTIC WIND; GUM NEBULA; IC 443;
ACCELERATION; EMISSION; SHOCK; DISCOVERY; REACCELERATION
AB The origin of Galactic cosmic-ray ions has remained an enigma for almost a century. Although it has generally been thought that they are accelerated in the shock waves associated with powerful supernova explosions-for which there have been recent claims of evidence-the mystery is far from resolved. In fact, we may be on the wrong track altogether in looking for isolated regions of cosmic-ray acceleration.
C1 Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA 02138 USA.
RP Butt, Y (reprint author), Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ybutt@cfa.harvard.edu
FU NASA Long Term Space Astrophysics
FX Part of this work was carried out while the author was a fellow at the
National Academy of Sciences. The support of a NASA Long Term Space
Astrophysics grant is gratefully acknowledged.
NR 46
TC 63
Z9 63
U1 0
U2 4
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 AUG 6
PY 2009
VL 460
IS 7256
BP 701
EP 704
DI 10.1038/nature08127
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 479OO
UT WOS:000268670300030
PM 19661909
ER
PT J
AU Norrbom, AL
Korytkowski, CA
AF Norrbom, Allen L.
Korytkowski, Cheslavo A.
TI A revision of the Anastrepha robusta species group (Diptera:
Tephritidae)
SO ZOOTAXA
LA English
DT Article
DE Anastrepha; Tephritidae; fruit flies; taxonomy; Polygalaceae; Moutabea
ID TROPICAL RAIN-FOREST; MEXICO; FLIES
AB The Anastrepha robusta species group is revised to include the following 29 species: A. amaryllis Tigrero (Ecuador), A. amazonensis, n. sp. (Brazil: Amazonas), A. bella, n. sp. (Panama), A. binodosa Stone (Brazil: Amazonas, Para), A. concava Greene (Costa Rica to Ecuador and Brazil: Amazonia), A. cordata Aldrich (Mexico to Venezuela), A. cryptostrepha Hendel (Peru, Surinam), A. cryptostrephoides, n. sp. (Peru), A. disticrux, n. sp. (Jamaica), A. fenestrata Lutz & Lima (Brazil: Amazonas, Para), A. fenestrella, n. sp. (Costa Rica, Panama), A. furcata Lima (Panama, French Guiana, Brazil: Amazonas, Para, Bahia, Espirito Santo), A. fuscata, n. sp. (Peru), A. isolata, n. sp. (Ecuador, Brazil: Amazonas), A. jamaicensis, n. sp. (Jamaica), A. lambda Hendel (Per), A. miza, n. sp. (Venezuela), A. nigra, n. sp. (Panama), A. nigrifascia Stone (Bahamas, USA: Florida), A. nigrivittata, n. sp. (Guyana), A. partita, n. sp. ("Amazon"), A. phaeoptera Lima (Brazil: Bahia, Rio Grande do Sul), A. pittieri Caraballo (Panama, Venezuela), A. pseudorobusta, n. sp. (Per, Trinidad, Venezuela), A. rafaeli, n. sp. (Brazil: Roraima, Venezuela), A. robusta Greene (Mexico to Panama), A. rojasi, n. sp. (Costa Rica, Panama), A. simulans Zucchi (Brazil: Parana, Sao Paulo, Rio de Janeiro), and A. speciosa Stone (Panama). Moutabea longifolia is recorded as a host plant of A. rojasi, the first host record for Anastrepha species from the plant family Polygalaceae. The larvae feed on the seeds within the fruit. A key to the species and descriptions and illustrations for each species are provided, and their possible relationships are discussed.
C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA.
[Korytkowski, Cheslavo A.] Univ Panama, Programa Maestria Entomol Vice Rectoria Invest &, Panama City, Panama.
RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM allen.norrbom@ars.usda.gov; cheslavok@cableonda.net
FU USDA [CS-ARS-6, FG-CR-107]
FX We sincerely thank the many scientists, curators and institutions who
kindly loaned or provided specimens for study, particularly Ian White
and John Chainey (BMNH), Norm Penny (CAS), Chen Young (CMP), Jeff
Cumming (CNC), Gary Steck (FSCA), Laszlo Papp (HNHM), Manuel Zumbado
(INBio), J. A. Rafael (INPA), C. J. Rosales (IZAM), Phil Perkins (MCZ),
Nancy Carrejo (MEUV), Chica do Val (MZUSP), Ruth Contreras-Lichtenberg
(NMW), Norma Nolazco (SENASA), Uwe Kallweit (SMT), Claudio Carvalho
(UFPC), and Wilford Hanson (USU). Many of the specimens from Costa Rica
were collected or reared by INBio parataxonomists supported by the
Research and Scientific Exchanges Division, Foreign Agricultural
Service, USDA (Project No. CS-ARS-6, Grant No. FG-CR-107). We are
grateful to Juan Tigrero for providing measurements and images of the
holotype of A. amaryllis. George Venable, Roy Larimer, Taina Litwak, and
Marie Metz produced some of the illustrations, and Terrence Walters
(USDA, APHIS, CPHST) secured funding for some of the illustration work.
We also thank Lucrecia Rodriguez for assistance with the illustrations,
and John Brown, Wayne Mathis, and Norman Woodley for their comments on
previous drafts of the manuscript.
NR 51
TC 19
Z9 19
U1 1
U2 2
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD AUG 6
PY 2009
IS 2182
BP 1
EP 91
PG 91
WC Zoology
SC Zoology
GA 480VP
UT WOS:000268765400001
ER
PT J
AU Hollingsworth, PM
Forrest, LL
Spouge, JL
Hajibabaei, M
Ratnasingham, S
van der Bank, M
Chase, MW
Cowan, RS
Erickson, DL
Fazekas, AJ
Graham, SW
James, KE
Kim, KJ
Kress, WJ
Schneider, H
van AlphenStahl, J
Barrett, SCH
van den Berg, C
Bogarin, D
Burgess, KS
Cameron, KM
Carine, M
Chacon, J
Clark, A
Clarkson, JJ
Conrad, F
Devey, DS
Ford, CS
Hedderson, TAJ
Hollingsworth, ML
Husband, BC
Kelly, LJ
Kesanakurti, PR
Kim, JS
Kim, YD
Lahaye, R
Lee, HL
Long, DG
Madrinan, S
Maurin, O
Meusnier, I
Newmaster, SG
Park, CW
Percy, DM
Petersen, G
Richardson, JE
Salazar, GA
Savolainen, V
Seberg, O
Wilkinson, MJ
Yi, DK
Little, DP
AF Hollingsworth, Peter M.
Forrest, Laura L.
Spouge, John L.
Hajibabaei, Mehrdad
Ratnasingham, Sujeevan
van der Bank, Michelle
Chase, Mark W.
Cowan, Robyn S.
Erickson, David L.
Fazekas, Aron J.
Graham, Sean W.
James, Karen E.
Kim, Ki-Joong
Kress, W. John
Schneider, Harald
van AlphenStahl, Jonathan
Barrett, Spencer C. H.
van den Berg, Cassio
Bogarin, Diego
Burgess, Kevin S.
Cameron, Kenneth M.
Carine, Mark
Chacon, Juliana
Clark, Alexandra
Clarkson, James J.
Conrad, Ferozah
Devey, Dion S.
Ford, Caroline S.
Hedderson, Terry A. J.
Hollingsworth, Michelle L.
Husband, Brian C.
Kelly, Laura J.
Kesanakurti, Prasad R.
Kim, Jung Sung
Kim, Young-Dong
Lahaye, Renaud
Lee, Hae-Lim
Long, David G.
Madrinan, Santiago
Maurin, Olivier
Meusnier, Isabelle
Newmaster, Steven G.
Park, Chong-Wook
Percy, Diana M.
Petersen, Gitte
Richardson, James E.
Salazar, Gerardo A.
Savolainen, Vincent
Seberg, Ole
Wilkinson, Michael J.
Yi, Dong-Keun
Little, Damon P.
CA CBOL Plant Working Grp
TI A DNA barcode for land plants
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE matK; rbcL; species identification
ID REGIONS; LOCI
AB DNA barcoding involves sequencing a standard region of DNA as a tool for species identification. However, there has been no agreement on which region(s) should be used for barcoding land plants. To provide a community recommendation on a standard plant barcode, we have compared the performance of 7 leading candidate plastid DNA regions (atpF-atpH spacer, matK gene, rbcL gene, rpoB gene, rpoC1 gene, psbK-psbI spacer, and trnH-psbA spacer). Based on assessments of recoverability, sequence quality, and levels of species discrimination, we recommend the 2-locus combination of rbcL + matK as the plant barcode. This core 2-locus barcode will provide a universal framework for the routine use of DNA sequence data to identify specimens and contribute toward the discovery of overlooked species of land plants.
C1 [Hollingsworth, Peter M.; Forrest, Laura L.; Clark, Alexandra; Hollingsworth, Michelle L.; Kelly, Laura J.; Long, David G.; Richardson, James E.] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland.
[Spouge, John L.] NIH, Natl Ctr Biotechnol Informat, Natl Lib Med, Computat Biol Branch, Bethesda, MD 20894 USA.
[Hajibabaei, Mehrdad; Ratnasingham, Sujeevan; Meusnier, Isabelle] Univ Guelph, Biodivers Inst Ontario, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
[van der Bank, Michelle; Lahaye, Renaud; Maurin, Olivier] Univ Johannesburg, Dept Bot & Plant Biotechnol, ZA-2006 Johannesburg, South Africa.
[Chase, Mark W.; Cowan, Robyn S.; van AlphenStahl, Jonathan; Clark, Alexandra; Clarkson, James J.; Devey, Dion S.; Kelly, Laura J.; Savolainen, Vincent] Royal Bot Gardens, Richmond TW9 3DS, Surrey, England.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
[Fazekas, Aron J.; Husband, Brian C.; Kesanakurti, Prasad R.; Newmaster, Steven G.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
[Graham, Sean W.; Percy, Diana M.] Univ British Columbia, UBC Bot Garden & Ctr Plant Res, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada.
[Graham, Sean W.; Percy, Diana M.] Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada.
[James, Karen E.; Schneider, Harald; Carine, Mark] Nat Hist Museum, Dept Bot, London SW7 5BD, England.
[Kim, Ki-Joong; Kim, Jung Sung; Lee, Hae-Lim; Yi, Dong-Keun] Korea Univ, Sch Life Sci & Biotechnol, Seoul 136701, South Korea.
[Barrett, Spencer C. H.; Burgess, Kevin S.] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON M5S 3B2, Canada.
[van den Berg, Cassio] Univ Estadual Feira de Santana, Lab Sistemat Mol Plantas, Dept Ciencias Biol, BR-44031460 Feira De Santana, Bahia, Brazil.
[Burgess, Kevin S.] Columbus State Univ, Dept Biol, Columbus, GA 31907 USA.
[Bogarin, Diego] Univ Costa Rica, Cartago, Costa Rica.
[Cameron, Kenneth M.] Univ Wisconsin, Dept Bot, Madison, WI 53508 USA.
[Chacon, Juliana; Madrinan, Santiago] Univ Los Andes, Bogota, DC, Colombia.
[Conrad, Ferozah] Kirstenbosch Res Ctr, Leslie Hill Mol Systemat Lab, SANBI, ZA-7735 Cape Town, South Africa.
[Ford, Caroline S.; Wilkinson, Michael J.] Aberystwyth Univ, Inst Biol Environm & Rural Sci, Aberystwyth SY23 3DA, Dyfed, Wales.
[Hedderson, Terry A. J.] Univ Cape Town, Dept Bot, ZA-7700 Rondebosch, South Africa.
[Kim, Young-Dong] Hallym Univ, Dept Life Sci, Chunchon 200702, South Korea.
[Park, Chong-Wook] Seoul Natl Univ, Sch Biol Sci, Seoul 151742, South Korea.
[Petersen, Gitte; Seberg, Ole] Univ Copenhagen, Nat Hist Museum Denmark, DK-1307 Copenhagen K, Denmark.
[Salazar, Gerardo A.] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04510, DF, Mexico.
[Savolainen, Vincent] Imperial Coll London, Ascot SL5 7PY, Berks, England.
[Little, Damon P.] New York Bot Garden, Cullman Program Mol Systemat, Bronx, NY 10458 USA.
RP Hollingsworth, PM (reprint author), Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland.
EM P.Hollingsworth@rbge.org.uk
RI Madrinan, Santiago/A-1149-2010; Chacon Pinilla, Juliana/N-1123-2015;
Richardson, James-Edward/L-2768-2016; Chase, Mark /A-6642-2011;
Petersen, Gitte/H-1903-2011; Schneider, Harald/B-6681-2008; Seberg,
Ole/A-5111-2013; van den Berg, Cassio/B-8968-2008; Herbario Virtual,
Inct/J-8725-2013; Barrett, Spencer/M-3751-2013; Ratnasingham,
Sujeevan/G-9103-2014; Graham, Sean/L-3944-2014;
OI Madrinan, Santiago/0000-0002-0807-6523; Chacon Pinilla,
Juliana/0000-0003-3993-2553; Richardson,
James-Edward/0000-0001-9014-4865; Forrest, Laura/0000-0002-0235-9506;
Petersen, Gitte/0000-0002-2325-0059; Schneider,
Harald/0000-0002-4548-7268; Seberg, Ole/0000-0001-9675-4090; van den
Berg, Cassio/0000-0001-5028-0686; Graham, Sean/0000-0001-8209-5231;
Hollingsworth, Peter/0000-0003-0602-0654; Yi,
Dong-Keun/0000-0002-3988-323X
NR 24
TC 638
Z9 711
U1 25
U2 231
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD AUG 4
PY 2009
VL 106
IS 31
BP 12794
EP 12797
DI 10.1073/pnas.0905845106
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 479NT
UT WOS:000268667600043
ER
PT J
AU Horn, JW
Fisher, JB
Tomlinson, PB
Lewis, CE
Laubengayer, K
AF Horn, James W.
Fisher, Jack B.
Tomlinson, P. Barry
Lewis, Carl E.
Laubengayer, Karen
TI EVOLUTION OF LAMINA ANATOMY IN THE PALM FAMILY (ARECACEAE)
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Arecaceae; correlated evolution; epidermis; homoplasy; hypodermis;
lamina anatomy; leaf biomechanics; macroevolution; palm phylogeny;
venation architecture
ID HETEROBARIC LEAVES; LATERAL ORGANS; HISTOGENETIC OBSERVATIONS; PLICATION
INCEPTION; FRACTURE-TOUGHNESS; LEAFLET SEPARATION; PHOTOSYNTHESIS;
PHYLOGENY; VENATION; PLANTS
AB The unique properties of tree building in Arecaceae strongly constrain their architectural lability. Potentially compensating for this limitation, the extensive diversification of leaf anatomical structure within palms involves many characters whose alternate states may confer disparate mechanical or physiological capabilities. In the context of a recent global palm phylogeny, we analyzed the evolution of 10 such lamina anatomical characters and leaf morphology of 161 genera, conducting parsimony and maximum likelihood ancestral state reconstructions, as well as tests of correlated evolution. Lamina morphology evolves independently from anatomy. Although many characters do optimize as synapomorphic for major clades, anatomical evolution is highly homoplasious. Nevertheless, it is not random: analyses indicate the recurrent evolution of different cohorts of correlated character state,. Notable are two surface layer (epidermis and hypodermis) types: (1) a parallel-laminated type of rectangular epidermal cells with sinuous anticlinal walls, with fibers present in the hypodermis and (2) a cross-laminated type of hexagonal cells in both layers. Correlated with the cross-laminated type is a remarkable decrease in the volume fraction of fibers, accompanied by changes in the architecture and sheath cell type of the transverse veins. We discuss these and other major patterns of anatomical evolution in relation to their biomechanical and ecophysiological significance.
C1 [Horn, James W.; Fisher, Jack B.; Tomlinson, P. Barry; Lewis, Carl E.] Fairchild Trop Bot Garden, Coral Gables, FL 33156 USA.
[Tomlinson, P. Barry] Kampong Natl Trop Bot Gardens, Miami, FL 33133 USA.
[Tomlinson, P. Barry] Harvard Univ, Petersham, MA 01366 USA.
[Laubengayer, Karen] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
RP Horn, JW (reprint author), Smithsonian Inst, Dept Bot, POB 37012,NMNH MRC 0166, Washington, DC 20013 USA.
EM hornj@si.edu
FU NSF [0515683]; National Tropical Botanical Garden
FX Woodbury and FTBG volunteers provided herbarium Support. Research was
Supported in part by NSF award 0515683 and the Crum Professorship in
Tropical Botany of the National Tropical Botanical Garden.
NR 91
TC 27
Z9 32
U1 2
U2 20
PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
J9 AM J BOT
JI Am. J. Bot.
PD AUG
PY 2009
VL 96
IS 8
BP 1462
EP 1486
DI 10.3732/ajb.0800396
PG 25
WC Plant Sciences
SC Plant Sciences
GA 480UO
UT WOS:000268762600009
PM 21628293
ER
PT J
AU Wurdack, KJ
Davis, CC
AF Wurdack, Kenneth J.
Davis, Charles C.
TI MALPIGHIALES PHYLOGENETICS: GAINING GROUND ON ONE OF THE MOST
RECALCITRANT CLADES IN THE ANGIOSPERM TREE OF LIFE
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Review
DE Centroplacaceae; classification; low-copy nuclear gene; Malpighiales;
multigene analyses; Peridiscaceae; Rafflesiacae; rapid radiation
ID COMPARATIVE FLORAL STRUCTURE; NUCLEAR-DNA SEQUENCES; HOLOPARASITIC
FLOWERING PLANTS; ANCIENT RAPID RADIATIONS; EUPHORBIACEAE-SENSU-LATO;
LONG-BRANCH ATTRACTION; SIEVE-ELEMENT PLASTIDS; CHAIN MONTE-CARLO;
GROUP-II INTRON; LARGE DATA SETS
AB The eudicot order Malpighiales contains similar to 16000 species and is the most poorly resolved large rosid clade. To clarify phylogenetic relationships in the order, we used maximum likelihood, Bayesian, and parsimony analyses of DNA sequence data from 13 gene regions, totaling 15604 bp, and representing all three genomic compartments (i.e., plastid: atpB, matK, ndhF, and rbcL; mitochondrial: ccmB, cob, matR, nad1B-C, nad6, and rps3; and nuclear: I SS rDNA, PHYC and newly developed low-copy EMB2765). Our sampling of 190 taxa includes representatives from all families of Malpighiales. These data provide greatly increased Support for the recent additions of Aneulophus, Bhesa, Centroplacus, Ploiarium, and Rafflesiaceae to Malpighiales sister relations of Phyllanthaceae + Picrodendraceae, monophyly of Hypericaccae, and polyphyly of Clusiaceae. Oxalidales + Huaceae, followed by Celastrales are successive sisters to Malpighiales. Parasitic Rafflesiaceae, which produce the world's largest flowers, are confirmed as embedded within a paraphyletic Euphorbiaceae. Novel findings show a well-supported placement of Ctenolophonaccae with Erythroxylaceae + Rhizophoraceae, sister-group relationships of Bhesa + Centroplacus, and the exclusion of Medusandra from Malpighiales. New taxonomic circumscriptions include the addition of Bhesa to Centroplacaceae, Medusandra to Peridiscaceae (Saxifragales), Calophyllaceae applied to Clusiaceae subfamily Kielmeyeroideae, Peraceae applied to Euphorbiaceae sublamily Peroideae, and Huaceae included in Oxalidales.
C1 [Wurdack, Kenneth J.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
[Davis, Charles C.] Harvard Univ Herbaria, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
RP Wurdack, KJ (reprint author), Smithsonian Inst, Dept Bot, POB 37012 NMNH MRC 166, Washington, DC 20013 USA.
EM wurdackk@si.edu; cdavis@oeb.harvard.edu
NR 193
TC 135
Z9 148
U1 4
U2 37
PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
EI 1537-2197
J9 AM J BOT
JI Am. J. Bot.
PD AUG
PY 2009
VL 96
IS 8
BP 1551
EP 1570
DI 10.3732/ajb.0800207
PG 20
WC Plant Sciences
SC Plant Sciences
GA 480UO
UT WOS:000268762600016
PM 21628300
ER
PT J
AU Raboy, BE
Fontoura, T
AF Raboy, B. E.
Fontoura, T.
TI BROMELIAD USE IN WILD GOLDEN-HEADED LION TAMARINS (LEONTOPITHECUS
CHRYSOMELAS): CONTINUED EVIDENCE OF THEIR MUTUALLY BENEFICIAL
RELATIONSHIP
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Raboy, B. E.] Smithsonian Natl Zool Pk, Dept Conservat & Sci, Washington, DC 20008 USA.
[Fontoura, T.] Univ Estadual Santa Cruz, Santa Cruz, RJ, Brazil.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 43
BP 43
EP 43
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800044
ER
PT J
AU Bentley-Condit, V
Power, M
AF Bentley-Condit, V.
Power, M.
TI TANA RIVER, KENYA, YELLOW BABOON (PAPIO CYNOCEPHALUS) DIET: COMPARISON
OF NUTRITIONAL DATA FOR FOREST VS. SAVANNAH FOOD SPECIES
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Bentley-Condit, V.] Grinnell Coll, Dept Anthropol, Grinnell, IA 50112 USA.
[Power, M.] Smithsonian Inst, Natl Zool Pk, Conservat Ecol Ctr, Washington, DC 20008 USA.
NR 0
TC 0
Z9 0
U1 5
U2 9
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 50
BP 45
EP 45
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800051
ER
PT J
AU Becker, K
Dittus, W
Kumarasingha, R
Nurnberg, P
AF Becker, K.
Dittus, W.
Kumarasingha, R.
Nuernberg, P.
TI ASSESSMENT OF INBREEDING AVOIDANCE IN SOCIAL GROUPS OF TOQUE MACAQUES
WITH NON-DISPERSING MALES
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Becker, K.; Nuernberg, P.] Univ Cologne, CCG, D-50674 Cologne, Germany.
[Dittus, W.] Smithsonian Inst Primate Project, Kandy, Sri Lanka.
[Dittus, W.] Inst Fundamental Studies, Kandy, Sri Lanka.
[Dittus, W.] Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA.
[Kumarasingha, R.] Univ Peradeniya, Fac Vet Med & Anim Sci, Dept Vet Pathobiol, Peradeniya, Sri Lanka.
NR 0
TC 0
Z9 0
U1 0
U2 5
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 53
BP 46
EP 46
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800054
ER
PT J
AU Power, ML
Maslanka, M
AF Power, M. L.
Maslanka, M.
TI THE MILK COLLECTION OF THE SMITHSONIAN NATIONAL ZOOLOGICAL PARK
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Power, M. L.; Maslanka, M.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC 20013 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 52
BP 46
EP 46
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800053
ER
PT J
AU Dindo, M
Stoinski, T
Subiaul, F
Whiten, A
AF Dindo, M.
Stoinski, T.
Subiaul, F.
Whiten, A.
TI SOCIAL LEARNING AND DIFFUSION OF NOVEL FORAGING TASKS IN ORANGUTANS
(PONGO PYGMAEUS X PONGO ABELII)
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Dindo, M.; Subiaul, F.] George Washington Univ, Washington, DC 20052 USA.
[Stoinski, T.] Zoo Atlanta, Atlanta, GA USA.
[Whiten, A.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland.
[Dindo, M.; Subiaul, F.] Smithsonian Natl Zool Pk, Washington, DC USA.
NR 0
TC 1
Z9 1
U1 0
U2 8
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 59
BP 48
EP 48
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800060
ER
PT J
AU Oliveira, LC
Hankerson, S
Dietz, JM
Raboy, BE
AF Oliveira, L. C.
Hankerson, S.
Dietz, J. M.
Raboy, B. E.
TI KEY TREE SPECIES FOR THE GOLDEN-HEADED LION TAMARIN AND IMPLICATIONS FOR
SHADE-COCOA MANAGEMENT IN SOUTHERN BAHIA, BRAZIL
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Oliveira, L. C.; Hankerson, S.; Dietz, J. M.] Univ Maryland, College Pk, MD 20742 USA.
[Raboy, B. E.] Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol 4, Washington, DC 20008 USA.
RI Oliveira, Leonardo/G-1290-2012
OI Oliveira, Leonardo/0000-0002-1774-0713
NR 0
TC 0
Z9 0
U1 0
U2 1
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 93
BP 59
EP 59
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800094
ER
PT J
AU Power, ML
AF Power, M. L.
TI PROXIMATE NUTRIENT COMPOSITION OF CAPTIVE BABOON (PAPIO HAMADRYAS) MILK
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 32nd Annual Meeting of the American-Society-of-Primatologists
CY SEP 18-21, 2009
CL San Diego, CA
SP Amer Soc Primatol, San Diego Zoo, Mira Costa Coll
C1 [Power, M. L.] Smithsonian Natl Zool Pk, Conservat & Ecol Ctr, Nutr Lab, Washington, DC 20008 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2009
VL 71
MA 218
BP 101
EP 101
PG 1
WC Zoology
SC Zoology
GA 488SJ
UT WOS:000269369800219
ER
PT J
AU Brostoff, LB
Centeno, SA
Ropret, P
Bythrow, P
Pottier, F
AF Brostoff, L. B.
Centeno, S. A.
Ropret, P.
Bythrow, P.
Pottier, F.
TI Combined X-ray Diffraction and Raman Identification of Synthetic Organic
Pigments in Works of Art: From Powder Samples to Artists' Paints
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID CRYSTAL-STRUCTURE; QUINACRIDONE; SPECTRA; SPECTROSCOPY; 20TH-CENTURY;
VARNISHES; COLOR; MEDIA; DYES
AB X-ray diffraction (XRD) complemented by Raman spectroscopy analyses of synthetic organic pigments in powder samples, layered paint systems, and commercial artists' paints bound in acrylic, alkyd, and oil media are presented. The potential and limitations of the techniques to identify and characterize mixtures of these pigments, along with inorganic extenders, in works of art are exemplified and discussed. Stratified model paint systems that mimic the layering structure typically found in modern paintings are used to evaluate the effect of the mu XRD experimental parameters, as well as extenders or fillers commonly found in modern artists' paint formulations, on the quality of the patterns recorded in microsamples of paint. XRD is demonstrated for the first time to be an effective tool for the specific identification of synthetic organic pigment mixtures and fillers in acrylic and alkyd bound artists' paints, while the identification of these pigments by XRD in oil bound paints appears problematic. Detailed crystallographic information provided by XRD is shown to be complementary to molecular information provided by Raman analysis. The combined use of these techniques allows for more frequent unambiguous compound identification than would be possible using one technique alone.
C1 [Brostoff, L. B.] Lib Congress, Preservat Directorate, Preservat Res & Testing Div, Washington, DC 20540 USA.
[Centeno, S. A.] Metropolitan Museum Art, New York, NY 10028 USA.
[Ropret, P.] Inst Protect Cultural Heritage Slovenia, Restorat Ctr, Ljubljana 1000, Slovenia.
[Brostoff, L. B.; Ropret, P.; Bythrow, P.; Pottier, F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
RP Brostoff, LB (reprint author), Lib Congress, Preservat Directorate, Preservat Res & Testing Div, 101 Independence Ave SE, Washington, DC 20540 USA.
EM lbrostoff@loc.gov; silvia.centeno@metmuseum.org
OI Centeno, Silvia/0000-0002-8496-4426
NR 37
TC 16
Z9 16
U1 0
U2 25
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
J9 ANAL CHEM
JI Anal. Chem.
PD AUG 1
PY 2009
VL 81
IS 15
BP 6096
EP 6106
DI 10.1021/ac9004953
PG 11
WC Chemistry, Analytical
SC Chemistry
GA 476PV
UT WOS:000268455600020
ER
PT J
AU Inanez, JG
Speakman, RJ
Garrigos, JBI
Glascock, MD
AF Inanez, J. G.
Speakman, R. J.
Buxeda i Garrigos, J.
Glascock, M. D.
TI CHEMICAL CHARACTERIZATION OF TIN-LEAD GLAZED POTTERY FROM THE IBERIAN
PENINSULA AND THE CANARY ISLANDS: INITIAL STEPS TOWARD A BETTER
UNDERSTANDING OF SPANISH COLONIAL POTTERY IN THE AMERICAS*
SO ARCHAEOMETRY
LA English
DT Article
DE MAJOLICA; NEUTRON ACTIVATION ANALYSIS (NAA); PROVENANCE; MULTIVARIATE
STATISTICS; IBERIAN PENINSULA; CANARY ISLANDS
ID COMPOSITIONAL DATA; LOGRATIO ANALYSIS; CERAMICS; ARCHAEOMETRY;
PROVENANCE; DISTANCE; MEXICO; SPAIN
AB Majolica pottery was the most characteristic tableware produced in Europe during the Medieval and Renaissance periods. Because of the prestige and importance attributed to this ware, Spanish majolica was imported in vast quantities into the Americas during the Spanish Colonial period. A study of Spanish majolica was conducted on a set of 186 samples from the 10 primary majolica production centres on the Iberian Peninsula and 22 sherds from two early colonial archaeological sites on the Canary Islands. The samples were analysed by neutron activation analysis (NAA), and the resulting data were interpreted using an array of multivariate statistical approaches. Our results show a clear discrimination between different production centres, allowing a reliable provenance attribution of the sherds from the Canary Islands.
C1 [Inanez, J. G.; Speakman, R. J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Inanez, J. G.; Buxeda i Garrigos, J.] Univ Barcelona, Fac Geog & Hist, Cultura Mat & Arqueometria Univ Barcelona ARQUB, Barcelona 08001, Catalonia, Spain.
[Glascock, M. D.] Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA.
RP Inanez, JG (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
RI Buxeda i Garrigos, Jaume/E-7228-2014;
OI Buxeda i Garrigos, Jaume/0000-0001-6857-8448; Glascock, Michael
D./0000-0003-0686-7556; Inanez, Javier/0000-0002-1411-8099; Speakman,
Robert/0000-0003-2063-154X
FU European Community [ICA-3-CT-2002-10018]; Smithsonian Institution; Museu
de la Cermica de Barcelona; Museo Arqueologico de Sevilla; Museo Canario
(Las Palmas de Gran Canaria); Parque Arqueologico de la Cueva Pintada
(Galdar, Gran Canaria); Associacio Catalana de Terrissa i Cermica
Decorada; National Science Foundation [0504015]
FX This work forms part of the project 'Identification, recovery and
improvement of ancient Mediterranean ceramic manufacturing technologies
for the reproduction of ceramic artefacts of archaeological value
(CERAMED)', from the Research Directorate General, European Commission,
European Community (ICA-3-CT-2002-10018). Javier G. Inanez is also
indebted to the Smithsonian Institution postdoctoral fellowship
programme for its support. Authors also are indebted to the Museu de la
Cermica de Barcelona, Museo Arqueologico de Sevilla, Museo Canario (Las
Palmas de Gran Canaria) and Parque Arqueologico de la Cueva Pintada
(Galdar, Gran Canaria), Mr Sanchez Cabezudo and Josep A. Cerd from the
Associacio Catalana de Terrissa i Cermica Decorada for their
collaboration in providing the samples. Special thanks are extended to
Nicole Little for assistance with laboratory work at MURR and to Dan
Cole for assistance with the illustrations. The laboratory work at MURR
was supported in part by National Science Foundation grant no. 0504015.
NR 59
TC 7
Z9 7
U1 1
U2 14
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0003-813X
J9 ARCHAEOMETRY
JI Archaeometry
PD AUG
PY 2009
VL 51
BP 546
EP 567
DI 10.1111/j.1475-4754.2008.00431.x
PG 22
WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear;
Geosciences, Multidisciplinary
SC Archaeology; Chemistry; Geology
GA 466JH
UT WOS:000267656900002
ER
PT J
AU Foley, RJ
Chornock, R
Filippenko, AV
Ganeshalingam, M
Kirshner, RP
Li, WD
Cenko, SB
Challis, PJ
Friedman, AS
Modjaz, M
Silverman, JM
Wood-Vasey, WM
AF Foley, Ryan J.
Chornock, Ryan
Filippenko, Alexei V.
Ganeshalingam, Mohan
Kirshner, Robert P.
Li, Weidong
Cenko, S. Bradley
Challis, Peter J.
Friedman, Andrew S.
Modjaz, Maryam
Silverman, Jeffrey M.
Wood-Vasey, W. Michael
TI SN 2008ha: AN EXTREMELY LOW LUMINOSITY AND EXCEPTIONALLY LOW ENERGY
SUPERNOVA
SO ASTRONOMICAL JOURNAL
LA English
DT Review
DE galaxies: individual (UGC 12682); supernovae: general; supernovae:
individual (SN 1991bj, SN 2002cx, SN 2004gw, SN 2006hn, SN 2007J, SN
2008ha)
ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; IA SUPERNOVA; IC SUPERNOVAE;
WHITE-DWARF; STAR-FORMATION; LIGHT CURVES; EVOLUTION; SPECTROSCOPY;
EMISSION; CALIBRATION
AB We present ultraviolet, optical, and near-infrared photometry as well as optical spectra of the peculiar supernova (SN) 2008ha. SN 2008ha had a very low peak luminosity, reaching only M(V) = -14.2 mag, and low line velocities of only similar to 2000 km s(-1) near maximum brightness, indicating a very small kinetic energy per unit mass of ejecta. Spectroscopically, SN 2008ha is a member of the SN 2002cx-like class of SNe, a peculiar subclass of SNe Ia; however, SN 2008ha is the most extreme member, being significantly fainter and having lower line velocities than the typical member, which is already similar to 2 mag fainter and has line velocities similar to 5000 km s-1 smaller (near maximum brightness) than a normal SN Ia. SN 2008ha had a remarkably short rise time of only similar to 10 days, significantly shorter than either SN 2002cx-like objects (similar to 15 days) or normal SNe Ia (similar to 19.5 days). The bolometric light curve of SN 2008ha indicates that SN 2008ha peaked at L(peak) = (9.5 +/- 1.4) x 10(40) erg s(-1), making SN 2008ha perhaps the least luminous SN ever observed. From its peak luminosity and rise time, we infer that SN 2008ha generated (3.0 +/- 0.9) x 10(-3)M(circle dot) of (56)Ni, had a kinetic energy of similar to 2 x 10(48) erg, and ejected 0.15 M(circle dot) of material. The host galaxy of SN 2008ha has a luminosity, star formation rate, and metallicity similar to those of the Large magellanic Cloud. We classify three new (and one potential) members of the SN 2002cx-like class, expanding the sample to 14 (and one potential) members. The host-galaxy morphology distribution of the class is consistent with that of SNe Ia, Ib, Ic, and II. Several models for generating low-luminosity SNe can explain the observations of SN 2008ha; however, if a single model is to describe all SN 2002cx-like objects, deflagration of carbon-oxygen white dwarfs, with SN 2008ha being a partial deflagration and not unbinding the progenitor star, is preferred. The rate of SN 2008ha-like events is similar to 10% of the SN Ia rate, and in the upcoming era of transient surveys, several thousand similar objects may be discovered, suggesting that SN 2008ha may be the tip of a low-luminosity transient iceberg.
C1 [Kirshner, Robert P.; Challis, Peter J.; Friedman, Andrew S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chornock, Ryan; Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong; Cenko, S. Bradley; Modjaz, Maryam; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
EM rfoley@cfa.harvard.edu
RI Friedman, Andrew/I-4691-2013
OI Friedman, Andrew/0000-0003-1334-039X
FU W. M. Keck Foundation; NASA/Swift Guest Investigator Grant [NNG06GH50G];
Clay Fellowship; NSF grant [AST-0606772, AST-0607485]; Gary and Cynthia
Bengier; Richard and Rhoda Goldman Fund; TABASGO Foundation; Miller
Institute of Basic Research in Science at U. C. Berkeley
FX Based in part 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 US National
Science Foundation on behalf of the Gemini partnership: the NSF (United
States), the Science and Technology Facilities Council (United Kingdom),
the National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia e Tecnologia
(Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina). 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 (NASA); the
observatory was made possible by the generous financial support of the
W. M. Keck Foundation. We acknowledge the use of public data from the
Swift data archive. We have made use of the SUSPECT SN spectra archive.
We are grateful to the staffs at the Lick, Keck, Gemini, and Fred L.
Whipple Observatories for their dedicated services. KAIT was constructed
and supported by donations from Sun Microsystems, Inc., the
Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the
NSF, the University of California, the Sylvia & Jim Katzman Foundation,
and the TABASGO Foundation. PAIRITEL is operated by the Smithsonian
Astrophysical Observatory (SAO) and was made possible by a grant from
the Harvard University Milton Fund, the camera loan from the University
of Virginia, and the continued support of the SAO and UC Berkeley. The
PAIRITEL project is supported by NASA/Swift Guest Investigator Grant
NNG06GH50G. We are especially grateful to J. Bloom, D. Starr, C. Blake,
A. Szentgyorgyi, and M. Skrutskie for developing and maintaining
PAIRITEL and E. Falco and the Mt. Hopkins staff (W. Peters, R. Hutchins,
and T. Groner) for their continued assistance with PAIRITEL. R. J. F. is
supported by a Clay Fellowship. Supernova research at Harvard is
supported by NSF grant AST-0606772. A. V. F.'s supernova group at U. C.
Berkeley is supported by NSF grant AST-0607485, Gary and Cynthia
Bengier, the Richard and Rhoda Goldman Fund, and the TABASGO Foundation.
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 NASA. M. M. is supported by
a research fellowship from the Miller Institute of Basic Research in
Science at U. C. Berkeley.
NR 105
TC 120
Z9 121
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2009
VL 138
IS 2
BP 376
EP 391
DI 10.1088/0004-6256/138/2/376
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 470QG
UT WOS:000267992300005
ER
PT J
AU Schild, RE
Lovegrove, J
Protopapas, P
AF Schild, Rudolph E.
Lovegrove, Justin
Protopapas, Pavlos
TI REVERBERATION IN THE UV-OPTICAL CONTINUUM BRIGHTNESS FLUCTUATIONS OF
MACHO QUASAR 13.5962.237
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; quasars: individual (MACHO 13.5962.237)
ID ACTIVE GALACTIC NUCLEI; VARIABILITY; Q0957+561; WINDS; SIZE
AB We examine the nature of brightness fluctuations in the UV-Optical spectral region of an ordinary quasar with 894 optical brightness measurements made during the epoch 1993-1999. We find evidence for systematic trends having the character of a pattern of reverberations following an initial disturbance. The initial pulses have brightness increases of the order of 20% and pulse widths of 50 days, and the reverberations have typical amplitudes of 12% with longer mean pulse widths of the order of 80 days and pulse separations of an order of 90 days. The repeat pattern occurs over the same timescales whether the initial disturbance is a brightening or fading. The lags of the pulse trains are comparable to the lags seen previously in reverberation of the broad blueshifted emission lines following brightness disturbances in Seyfert galaxies, when allowance is made for the mass of the central object. In addition to the burst pulse trains, we find evidence for a semiperiodicity with a timescale of two years. These strong patterns of brightness fluctuations suggest a method of discovering quasars from photometric monitoring alone, with data of the quality expected from large brightness monitoring programs such as Pan-STARRS and LSST.
C1 [Schild, Rudolph E.; Lovegrove, Justin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lovegrove, Justin] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Protopapas, Pavlos] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA.
[Protopapas, Pavlos] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Schild, RE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rschild@cfa.harvard.edu
NR 17
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2009
VL 138
IS 2
BP 421
EP 427
DI 10.1088/0004-6256/138/2/421
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 470QG
UT WOS:000267992300008
ER
PT J
AU Strader, J
Smith, GH
Larsen, S
Brodie, JP
Huchra, JP
AF Strader, Jay
Smith, Graeme H.
Larsen, Soeren
Brodie, Jean P.
Huchra, John P.
TI MASS-TO-LIGHT RATIOS FOR M31 GLOBULAR CLUSTERS: AGE DATING AND A
SURPRISING METALLICITY TREND
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: star clusters; globular clusters: general
ID BLUE STRAGGLER STARS; FUNDAMENTAL PLANE; MILKY-WAY; STRUCTURAL
PARAMETERS; POPULATION SYNTHESIS; ELLIPTIC GALAXIES; YOUNG CLUSTERS;
DWARF GALAXIES; PHOTOMETRY; CATALOG
AB We have obtained velocity dispersions from Keck high-resolution integrated spectroscopy of 10M31 globular clusters (GCs), including three candidate intermediate-age GCs. We show that these candidates have the same V-band mass-to-light (M/L(V)) ratios as the other GCs, implying that they are likely to be old. We also find a trend of derived velocity dispersion with wavelength, but cannot distinguish between a systematic error and a physical effect. Our new measurements are combined with photometric and spectroscopic data from the literature in a re-analysis of all M31 GC M/L(V) values. In a combined sample of 27 GCs, we show that the metal-rich GCs have lower M/L(V) than the metal-poor GCs, in conflict with predictions from stellar population models. Fragmentary data for other galaxies support this observation. The M31 GC fundamental plane is extremely tight, and we follow up an earlier suggestion by Djorgovski to show that the fundamental plane can be used to estimate accurate distances (potentially 10% or better).
C1 [Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Smith, Graeme H.; Brodie, Jean P.] UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Larsen, Soeren] Univ Utrecht, Utrecht, Netherlands.
EM jstrader@cfa.harvard.edu
FU NASA [NAS5-26555]; NSF [AST-0808099]; Smithsonian Institution; NWO VIDI
[639.042.610]; W. M. Keck Foundation
FX We thank an anonymous referee for a critical reading of the manuscript.
J. S. was supported by NASA through a Hubble Fellowship, administered by
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. J. B. acknowledges support from the NSF
through grant AST-0808099. J. P. H. was supported by the Smithsonian
Institution. S. L. acknowledges support by NWO VIDI grant 639.042.610.
J. S. is indebted to Dave Latham for his hospitality when the paper was
being finished. 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 theNational Aeronautics and Space Administration. The Observatory
was made possible by the generous financial support of the W. M. Keck
Foundation. We acknowledge Steve Vogt and the entire HIRES team for
building an instrument with such excellent long-term stability.
NR 49
TC 32
Z9 32
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2009
VL 138
IS 2
BP 547
EP 557
DI 10.1088/0004-6256/138/2/547
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 470QG
UT WOS:000267992300022
ER
PT J
AU Bianco, FB
Protopapas, P
McLeod, BA
Alcock, CR
Holman, MJ
Lehner, MJ
AF Bianco, F. B.
Protopapas, P.
McLeod, B. A.
Alcock, C. R.
Holman, M. J.
Lehner, M. J.
TI A SEARCH FOR OCCULTATIONS OF BRIGHT STARS BY SMALL KUIPER BELT OBJECTS
USING MEGACAM ON THE MMT
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Kuiper Belt; solar system: formation
ID JUPITER-FAMILY COMETS; ATMOSPHERIC INTENSITY SCINTILLATION;
TRANS-NEPTUNIAN BODIES; OUTER SOLAR-SYSTEM; SIZE DISTRIBUTION; STELLAR
OCCULTATIONS; MILLISECOND DIPS; SURFACE AGE; SCO X-1; LIGHT
AB We conducted a search for occultations of bright stars by Kuiper Belt Objects (KBOs) to estimate the density of subkilometer KBOs in the sky. We report here the first results of this occultation survey of the outer solar system conducted in 2007 June and 2008 June/July at the MMT Observatory using Megacam, the large MMT optical imager. We used Megacam in a novel shutterless continuous-readout mode to achieve high-precision photometry at 200 Hz, which with point-spread function convolution results in an effective sampling of similar to 30 Hz. We present an analysis of 220 star hours of data at a signal-to-noise ratio of 25 or greater, taken from images of fields within 3. of the ecliptic plane. The survey efficiency is greater than 10% for occultations by KBOs of diameter d >= 0.7 km, and we report no detections in our data set. We set a new 95% confidence level upper limit for the surface density Sigma(N) (d) of KBOs larger than 1 km: Sigma(N) (d >= 1 km) <= 2.0 x 10(8) deg(-2), and for KBOs larger than 0.7 km Sigma(N) (d >= 0.7 km) <= 4.8 x 10(8) deg(-2).
C1 [Bianco, F. B.; Lehner, M. J.] Univ Penn, Philadelphia, PA 19104 USA.
[Bianco, F. B.; Protopapas, P.; McLeod, B. A.; Alcock, C. R.; Holman, M. J.; Lehner, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bianco, F. B.; Protopapas, P.] Initiat Innovat Comp Harvard, Cambridge, MA 02138 USA.
[Lehner, M. J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
RP Bianco, FB (reprint author), Univ Penn, 209 S 33rd St, Philadelphia, PA 19104 USA.
EM fbianco@cfa.harvard.edu
OI Lehner, Matthew/0000-0003-4077-0985
NR 46
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2009
VL 138
IS 2
BP 568
EP 578
DI 10.1088/0004-6256/138/2/568
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 470QG
UT WOS:000267992300024
ER
PT J
AU Meszaros, S
Avrett, EH
Dupree, AK
AF Meszaros, Sz.
Avrett, E. H.
Dupree, A. K.
TI MASS OUTFLOW FROM RED GIANT STARS IN M13, M15, AND M92
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE globular clusters: general; globular clusters: individual (M13, M15,
M92); stars: AGB and post-AGB; stars: chromospheres; stars: mass loss
ID SPACE-TELESCOPE OBSERVATIONS; GLOBULAR-CLUSTERS; CHROMOSPHERIC ACTIVITY;
INTRACLUSTER MEDIUM; COLOR-MAGNITUDE; MILKY-WAY; RGB STARS; POPULATION;
DUST; BRANCH
AB Chromospheric model calculations of the H alpha line for selected red giant branch and asymptotic giant branch (AGB) stars in the globular clusters M13, M15, and M92 are constructed to derive mass loss rates (MLRs). The model spectra are compared to the observations obtained with the Hectochelle on the MMT telescope. These stars show strong H alpha emissions and blueshifted H alpha cores signaling that mass outflow is present in all stars. Outflow velocities of 3-19 km s(-1), larger than indicated by H alpha profiles, are needed in the upper chromosphere to achieve good agreement between the model spectra and the observations. The resulting MLRs range from 0.6 x 10(-9) to 5 x 10(-9) M(circle dot) yr(-1), which are about an order of magnitude lower than predicted from "Reimers' law" or inferred from the infrared excess of similar stars. The MLR increases slightly with luminosity and with decreasing effective temperature. Stars in the more metal-rich M13 have higher MLRs by a factor of similar to 2 than in the metal-poor clusters M15 and M92. A fit to the MLRs is given by (M) over dot (M(circle dot) yr(-1)) = 0.092 x L(0.16) x T(eff)(-2.02) x A(0.37), where A = 10([Fe/H]). Multiple observations of stars revealed one object in M15, K757, in which the mass outflow increased by a factor of 6 between two observations separated by 18 months. Other stars showed changes in MLR by a factor of 1.5 or less.
C1 [Meszaros, Sz.] Univ Szeged, Dept Opt & Quantum Elect, H-6071 Szeged, Hungary.
[Avrett, E. H.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Meszaros, S (reprint author), Univ Szeged, Dept Opt & Quantum Elect, H-6071 Szeged, Hungary.
EM meszi@physx.u-szeged.hu; eavrett@cfa.harvard.edu; dupree@cfa.harvard.edu
RI Meszaros, Szabolcs/N-2287-2014
OI Meszaros, Szabolcs/0000-0001-8237-5209
FU SAO Predoctoral Fellowship; NASA; Hungarian OTKA [K76816]; Smithsonian
Astrophysical Observatory
FX We are grateful to Rudi Loeser who was instrumental in developing the
PANDORA code. We thank Bob Kurucz for help with the model photospheres.
S. M. is supported in part by an SAO Predoctoral Fellowship, NASA, and
the Hungarian OTKA Grant K76816. This research is also supported in part
by the Smithsonian Astrophysical Observatory.
NR 42
TC 29
Z9 29
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2009
VL 138
IS 2
BP 615
EP 624
DI 10.1088/0004-6256/138/2/615
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 470QG
UT WOS:000267992300028
ER
PT J
AU Grupp, F
Kurucz, RL
Tan, K
AF Grupp, F.
Kurucz, R. L.
Tan, K.
TI New extended atomic data in cool star model atmospheres Using Kurucz's
new iron data in MAFAGS-OS models
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atomic data; Sun: abundances; stars: abundances; stars: atmospheres;
stars: fundamental parameters; stars: late-type
ID NEARBY STARS; TURBULENT CONVECTION; GALACTIC DISK; HALO; PROJECT
AB Context. Cool star model atmospheres are a common tool for the investigation of stellar masses, ages and elemental abundance composition. Theoretical atmospheric models strongly depend on the atomic data used when calculating them.
Aims. We present the changes in flux and temperature stratification when changing from iron data computed by R.L. Kurucz in the mid 90s to the Kurucz 2009 iron computations.
Methods. MAFAGS-OS opacity sampling atmospheres were recomputed with Kurucz 2009 iron atomic data as implemented in the VALD database by Ryabchikova. Temperature stratification and emergent flux distribution of the new version, called MAFAGS-OS9, is compared to the former version and to solar flux measurements.
Results. Using the Kurucz line lists converted into the VALD format and new bound-free opacities for Mg I and Al I leads to changes in the solar temperature stratification by not more than 28 K. At the same time, the calculated solar flux distribution shows significantly better agreement between observations and theoretical solar models. These changes in the temperature stratification of the corresponding models are small, but nevertheless of a magnitude that affects stellar parameter determinations and abundance analysis.
C1 [Grupp, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Grupp, F.] Univ Sternwarte, D-81679 Munich, Germany.
[Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tan, K.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
RP Grupp, F (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM frank@grupp-astro.de; rkurucz@cfa.harvard.edu; tan@bao.ac.cn
FU German Deutsche Forschungsgemeinschaft, DFG [Ge 490/31-1]; National
Natural Science Foundation of China [10521001, 10433010]; National Basic
Research Program of China (973 Program) [2007CB815103]
FX Part of this work was supported by the German Deutsche
Forschungsgemeinschaft, DFG project number Ge 490/31-1, by the National
Natural Science Foundation of China under Grants No. 10521001 and
10433010 and by the National Basic Research Program of China (973
Program) under Grant No. 2007CB815103.
NR 35
TC 22
Z9 22
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 503
IS 1
BP 177
EP 181
DI 10.1051/0004-6361/200912302
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 485UM
UT WOS:000269150300020
ER
PT J
AU Caramazza, M
Drake, JJ
Micela, G
Flaccomio, E
AF Caramazza, M.
Drake, J. J.
Micela, G.
Flaccomio, E.
TI Hard X-ray flux from low-mass stars in the Cygnus OB2 association
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: coronae; stars: flare; Galaxy: open clusters and associations:
individual: Cygnus OB2
ID SOLAR-FLARES; PROTOPLANETARY DISKS; EXTREME-ULTRAVIOLET; EMISSION;
STELLAR; BEPPOSAX; IONIZATION; MICROFLARES; CORONAE; MISSION
AB Context. The Cygnus OB2 association, the central engine of the Cygnus X star-forming region, is the subject of an extensive INTEGRAL Key Project that will accumulate 6Ms of observations. Analysis of 2Ms of observations by De Becker and co-workers provides the most sensitive limit yet obtained on hard X-ray emission from the cluster.
Aims. We investigate the X-ray emission in the 20-40 keV band expected from the flaring low-mass stellar population in Cygnus OB2. We discuss whether such emission needs to be considered in the interpretation of existing and future X-ray observations of the region, and whether such observations might provide insight into the high-energy processes on low-mass pre-main sequence stars.
Methods. The total hard X-ray flux from low-mass stars is estimated by assuming the observed soft X-ray emission stems from a superposition of flares. We further assume the ratio of hard X-ray to soft X-ray emission is described by a scaling found for solar flares by Isola and co-workers.
Results. We estimate the low-mass stellar hard X-ray flux in the 20-40 keV band to lie in the range similar to 2 x 10(31)-6 x 10(32) erg s(-1) and discuss some potential biases that might affect this result.
Conclusions. Hard X-ray emission could lie at a level not much below the current observed flux upper limits for Cygnus OB2. If this emission could be detected, it would provide insight into the hard X-ray production of large flares on pre-main sequence stars. We highlight the penetrating power of hard X-rays from low-mass stellar populations as a possible pointer to our Galaxy's hidden star-forming clusters and super-clusters using more sensitive observations from future missions.
C1 [Caramazza, M.] Univ Palermo, Dipartimento Sci Fis & Astron, I-90123 Palermo, Italy.
[Caramazza, M.; Micela, G.; Flaccomio, E.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
[Drake, J. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Caramazza, M (reprint author), Univ Palermo, Dipartimento Sci Fis & Astron, Via Archirafi 36, I-90123 Palermo, Italy.
EM mcarama@astropa.unipa.it; jdrake@cfa.harvard.edu;
giusi@astropa.unipa.it; flaccomio@astropa.unipa.it
FU NASA [NAS8-39073]; Chandra X-ray Center (CXC); ISHERPA program;
Ministero dell' Universta e della Ricerca and ASI/INAF [I/023/05/0]
FX J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray
Center (CXC) during the course of this research and thanks the CXC
director, Harvey Tananbaum, and the CXC science team for advice and
support. J.J.D. also thanks the ISHERPA program for financial support
during his visit to the Osservatorio Astronomico di Palermo, and the
Osservatorio director, Prof. S. Sciortino, and sta. for their help and
warm hospitality. M. C., G. M. and E. F. acknowledge financial support
from the Ministero dell' Universta e della Ricerca and ASI/INAF Contract
I/023/05/0. J.J.D. thanks Jurgen Knodlseder for useful discussions that
partly inspired this work. The authors thank the referee Manuel Gudel
for suggestions and useful comments that improved this work.
NR 45
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 503
IS 2
BP 505
EP 509
DI 10.1051/0004-6361/200811342
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HE
UT WOS:000269726200019
ER
PT J
AU Barbieri, M
Alonso, R
Desidera, S
Sozzetti, A
Fiorenzano, AFM
Almenara, JM
Cecconi, M
Claudi, RU
Charbonneau, D
Endl, M
Granata, V
Gratton, R
Laughlin, G
Loeillet, B
AF Barbieri, M.
Alonso, R.
Desidera, S.
Sozzetti, A.
Martinez Fiorenzano, A. F.
Almenara, J. M.
Cecconi, M.
Claudi, R. U.
Charbonneau, D.
Endl, M.
Granata, V.
Gratton, R.
Laughlin, G.
Loeillet, B.
CA Exoplanet Amateur Consortium
TI Characterization of the HD 17156 planetary system
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: individual: HD 17156; stars: binaries: eclipsing; stars:
planetary systems; techniques: spectroscopic; techniques: photometric
ID MASS-LUMINOSITY-RELATION; TRANSITING PLANET; EXTRASOLAR PLANETS; PARENT
STARS; SPIN-ORBIT; ECCENTRIC ORBIT; EVOLVED STARS; GIANT PLANET; LIGHT
CURVES; HOST STARS
AB Aims. We present data to improve the known parameters of the HD 17156 system (peculiar due to the eccentricity and long orbital period of its transiting planet) and constrain the presence of stellar companions.
Methods. Photometric data were acquired for 4 transits, and high precision radial velocity measurements were simultaneously acquired with the SARG spectrograph at TNG for one transit. The template spectra of HD 17156 was used to derive effective temperature, gravity, and metallicity. A fit of the photometric and spectroscopic data was performed to measure the stellar and planetary radii, and the spin-orbit alignment. Planet orbital elements and ephemeris were derived from the fit. Near infrared adaptive optic images were acquired with the AdOpt module of TNG.
Results. We found that the star has a radius of R(S) = 1.44 +/- 0.03 R(circle dot) and the planet R(P) = 1.02 +/- 0.08 R(J). The transit ephemeris is T(c) = 2 454 756.73134 +/- 0.00020 + N . 21.21663 +/- 0.00045 BJD. Analysis of the Rossiter-Mclaughlin effect shows that the system is spin orbit aligned with an angle beta = 4.8 degrees +/- 5.3 degrees. The analysis of high resolution images did not reveal any stellar companion with a projected separation between of 150 and 1 000 AU from HD 17156.
C1 [Barbieri, M.; Alonso, R.; Loeillet, B.] Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Desidera, S.; Claudi, R. U.; Granata, V.; Gratton, R.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Sozzetti, A.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Martinez Fiorenzano, A. F.; Cecconi, M.] INAF, Fdn Galileo Galilei, Brena Baja 38712, TF, Spain.
[Almenara, J. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Loeillet, B.] IAP, F-75014 Paris, France.
[Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Endl, M.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Granata, V.] Univ Padua, CISAS, I-35100 Padua, Italy.
[Laughlin, G.] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA.
RP Barbieri, M (reprint author), Lab Astrophys Marseille, 38 Rue Joliot Curie, F-13388 Marseille 13, France.
EM mauro.barbieri@oamp.fr
RI Alonso, Roi/D-8799-2014;
OI Alonso, Roi/0000-0001-8462-8126; Desidera, Silvano/0000-0001-8613-2589;
Sozzetti, Alessandro/0000-0002-7504-365X; GRANATA,
Valentina/0000-0002-1425-4541; Barbieri, Mauro/0000-0001-8362-3462;
Gratton, Raffaele/0000-0003-2195-6805
FU PRIN
FX This work was partially funded by PRIN 2006 "From disk to planetary
systems: understanding the origin and demographics of solar and
extrasolar planetary systems" by INAF. We thank the TNG director for
time allocation in Director Discretionary Time. We thank the referre
Norio Narita for his useful comments and suggestions.
NR 68
TC 22
Z9 22
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 503
IS 2
BP 601
EP 612
DI 10.1051/0004-6361/200811466
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HE
UT WOS:000269726200031
ER
PT J
AU Pietrukowicz, P
Minniti, D
Fernandez, JM
Pietrzynski, G
Ruiz, MT
Gieren, W
Diaz, RF
Zoccali, M
Hempel, M
AF Pietrukowicz, P.
Minniti, D.
Fernandez, J. M.
Pietrzynski, G.
Ruiz, M. T.
Gieren, W.
Diaz, R. F.
Zoccali, M.
Hempel, M.
TI Deep census of variable stars in a VLT/VIMOS field in Carina
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: variables: general; stars: variables: delta Sct; binaries:
eclipsing; stars: flare; planetary systems; stars: statistics
ID EXTRASOLAR PLANETARY CANDIDATES; GRAVITATIONAL LENSING EXPERIMENT;
LUMINOSITY OBJECT TRANSITS; MILLIMAGNITUDE PHOTOMETRY; ECLIPSING BINARY;
PERIOD SEARCH; CEPHEID; CATALOG; BULGE
AB Aims. We searched for variable stars in deep V-band images of a field towards the Galactic plane in Carina.
Methods. The images were taken with the VIMOS instrument at ESO VLT during 4 contiguous nights in April 2005. We detected 348 variables among 50 897 stars in the magnitude range between V = 15.4 and V = 24.5 mag. After detection, we classified the variables by a direct eye inspection of their light curves.
Results. All variable objects besides 9 OGLE transits in the field are new discoveries. We provide a complete catalog of all variables, which includes eclipsing/ellipsoidal binaries, miscellaneous pulsators (mostly delta Scuti-type variables), stars with flares, and other (irregular and likely long-period) variables. Only two of the stars in our sample are known to host planets.
Conclusions. Our result has implications for future large variability surveys.
C1 [Pietrukowicz, P.; Minniti, D.; Fernandez, J. M.; Zoccali, M.; Hempel, M.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Pietrukowicz, P.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Minniti, D.] Vatican Observ, V-00120 Vatican City, Vatican.
[Fernandez, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pietrzynski, G.; Gieren, W.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Pietrzynski, G.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Ruiz, M. T.] Univ Chile, Dept Astron, Santiago, Chile.
[Diaz, R. F.] CONICET UBA, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
RP Pietrukowicz, P (reprint author), Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Av Vicuna MacKenna 4860,Casilla 306, Santiago 22, Chile.
EM pietruk@astro.puc.cl
RI Diaz, Rodrigo/H-1487-2011; Ruiz, Maria Teresa/I-5770-2016;
OI Ruiz, Maria Teresa/0000-0002-6799-1537; Diaz,
Rodrigo/0000-0001-9289-5160
FU FONDAP Center for Astrophysics [15010003]; BASAL Center for Astrophysics
and Associated Technologies [PFB06]; Foundation for Polish Science;
Proyecto FONDECYT [1085278, 2090213]
FX P.P., D.M., J.M.F., G.P., M.T.R., W.G., M.H. are supported by FONDAP
Center for Astrophysics No. 15010003 and BASAL Center for Astrophysics
and Associated Technologies PFB06. P.P. was also supported by the
Foundation for Polish Science through program MISTRZ. M.Z. and D. M.
acknowledge support by Proyecto FONDECYT Regular No. 1085278 and
2090213, respectively. We are grateful to the ESO staff at Paranal
Observatory.
NR 36
TC 7
Z9 7
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 503
IS 2
BP 651
EP 662
DI 10.1051/0004-6361/200912142
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HE
UT WOS:000269726200036
ER
PT J
AU Bruderer, S
Benz, AO
Bourke, TL
Doty, SD
AF Bruderer, S.
Benz, A. O.
Bourke, T. L.
Doty, S. D.
TI Evidence of warm and dense material along the outflow of a high-mass YSO
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: molecules; stars: individual: AFGL 2591
ID YOUNG STELLAR OBJECTS; PHOTODISSOCIATION REGIONS; CHEMISTRY; ENVELOPE;
INTERFEROMETRY; RADIATION; AFGL-2591
AB Context. Outflow cavities in envelopes of young stellar objects (YSOs) have been predicted to allow far-UV (FUV) photons to escape far from the central source, with significant observable effects, especially if the protostar is a forming high-mass star suspected of emitting a copious amount of FUV radiation. Indirect evidence of this picture has been provided by models and unresolved single-dish observations, but direct high-resolution data are necessary for confirmation. Previous chemical modeling has suggested that CS and HCN are good probes of the local FUV field, so make good target species.
Aims. We directly probe the physical conditions of the material in the outflow walls to test this prediction.
Methods. Interferometric observations of the CS(7-6) and HCN(4-3) rotational lines in the high-mass star-forming region AFGL 2591 are carried out in the compact and extended configuration of the SubMillimeter Array (SMA). The velocity structure was analyzed, and integrated maps compared to K-band near-IR observations. A chemical model predicts abundances of CS and HCN for a gas under protostellar X-ray and FUV irradiation, and was used in conjunction with the data to distinguish between physical scenarios.
Results. CS and HCN emission was found in spatial coincidence in extended sources displaced up to 7 '' from the position of the young star. Their line widths are small, excluding major shocks. Chemical model calculations predict an enhanced abundance of the two molecules in warm, dense, and FUV irradiated gas. Hot dust observed between the molecular emission and the outflow accounts for the necessary attenuation to prevent photodissociation of the molecules.
Conclusions. The SMA data suggest that the outflow walls are heated and chemically altered by the FUV emission of the central high-mass object, providing the best direct evidence yet of large-scale direct irradiation of outflow walls.
C1 [Bruderer, S.; Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA.
RP Bruderer, S (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland.
EM simonbr@astro.phys.ethz.ch
FU Swiss National Science Foundation [200020-113556 (SB)]; The Research
Corporation (SDD); NASA [NNX08AH28G]
FX We thank Cecilia Ceccarelli, Michael Meyer, Michael Rissi, and Pascal
Stauber for useful discussions. The work was supported by the Swiss
National Science Foundation grant 200020-113556 (SB), a grant from The
Research Corporation (SDD) and the NASA grant NNX08AH28G (SDD). This
work makes use of observations obtained at the Gemini Observatory
(acquired through the Gemini Science Archive), 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.
NR 14
TC 10
Z9 10
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 503
IS 2
BP L13
EP U9
DI 10.1051/0004-6361/200912620
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 493HE
UT WOS:000269726200001
ER
PT J
AU Pont, F
Hebrard, G
Irwin, JM
Bouchy, F
Moutou, C
Ehrenreich, D
Guillot, T
Aigrain, S
Bonfils, X
Berta, Z
Boisse, I
Burke, C
Charbonneau, D
Delfosse, X
Desort, M
Eggenberger, A
Forveille, T
Lagrange, AM
Lovis, C
Nutzman, P
Pepe, F
Perrier, C
Queloz, D
Santos, NC
Segransan, D
Udry, S
Vidal-Madjar, A
AF Pont, F.
Hebrard, G.
Irwin, J. M.
Bouchy, F.
Moutou, C.
Ehrenreich, D.
Guillot, T.
Aigrain, S.
Bonfils, X.
Berta, Z.
Boisse, I.
Burke, C.
Charbonneau, D.
Delfosse, X.
Desort, M.
Eggenberger, A.
Forveille, T.
Lagrange, A. -M.
Lovis, C.
Nutzman, P.
Pepe, F.
Perrier, C.
Queloz, D.
Santos, N. C.
Segransan, D.
Udry, S.
Vidal-Madjar, A.
TI Spin-orbit misalignment in the HD80606 planetary system
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: planetary systems
ID GIANT PLANETS; LIGHT CURVES; METALLICITY; EXOPLANETS; SCINTILLATION;
DWARFS; SEARCH
AB We recently reported the photometric and spectroscopic detection of the primary transit of the 111-day-period, eccentric extra-solar planet HD80606b, at Observatoire de Haute-Provence, France. The whole egress of the primary transit and a section of its central part were observed, allowing the measurement of the planetary radius, and evidence for a spin-orbit misalignment through the observation of the Rossiter-McLaughlin anomaly. The ingress not having been observed for this long-duration transit, uncertainties remained in the parameters of the system. We present here a refined, combined analysis of our photometric and spectroscopic data, together with further published radial velocities, ground-based photometry, and Spitzer photometry around the secondary eclipse, as well as new photometric measurements of HD80606 acquired at Mount Hopkins, Arizona, just before the beginning of the primary transit. Although the transit is not detected in those new data, they provide an upper limit for the transit duration, which narrows down the possible behaviour of the Rossiter-McLaughlin anomaly in the unobserved part of the transit. We analyse the whole data with a Bayesian approach using a Markov-chain Monte Carlo integration on all available information. We find R(p) = 0.98 +/- 0.03 R(Jup) for the planetary radius, and a total primary transit duration of 11.9 +/- 1.3 h from first to fourth contact. Our analysis reinforces the hypothesis of spin-orbit misalignment in this system (alignment excluded at >95% level), with a positive projected angle between the planetary orbital axis and the stellar rotation (median solution lambda similar to 50 degrees). As HD80606 is a component of a binary system, the peculiar orbit of its planet could result from a Kozai mechanism.
C1 [Pont, F.; Aigrain, S.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Hebrard, G.; Bouchy, F.; Boisse, I.; Vidal-Madjar, A.] Univ Paris 06, CNRS, Inst Astrophys, UMR7095, F-75014 Paris, France.
[Irwin, J. M.; Nutzman, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bouchy, F.; Berta, Z.; Charbonneau, D.] Observ Haute Provence, F-04870 St Michel lObservatoire, France.
[Moutou, C.] CNRS Provence, Astrophys Lab, UMR 6110, F-13388 Marseille 13, France.
[Moutou, C.] Univ Aix Marseille 1, F-13388 Marseille 13, France.
[Ehrenreich, D.; Bonfils, X.; Delfosse, X.; Desort, M.; Eggenberger, A.; Forveille, T.; Lagrange, A. -M.; Perrier, C.] Univ Grenoble 1, Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France.
[Guillot, T.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, UMR 6202, F-06304 Nice 4, France.
[Lovis, C.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Burke, C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Pont, F (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
EM fpont@astro.ex.ac.uk
RI Santos, Nuno/E-9957-2011;
OI Santos, Nuno/0000-0003-4422-2919; Boisse, Isabelle/0000-0001-8388-8399;
Berta-Thompson, Zachory/0000-0002-3321-4924; Ehrenreich,
David/0000-0001-9704-5405
FU "Programme national de planetologie" (PNP) of CNRS/INSU, France; Swiss
National Science Foundation (FNSRS); UK Science and Technology
Facilities Council; French CNRS; Fundacao para a Ciencia e a Tecnologia,
Portugal; David and Lucile Packard Fellowship for Science and
Engineering; US National Science Foundation [AST-0807690]
FX Financial support for the SOPHIE Consortium from the "Programme national
de planetologie" (PNP) of CNRS/INSU, France, and from the Swiss National
Science Foundation (FNSRS) are gratefully acknowledged. We also
acknowledge support from the UK Science and Technology Facilities
Council, the French CNRS and Fundacao para a Ciencia e a Tecnologia,
Portugal. The MEarth team gratefully acknowledges funding from the David
and Lucile Packard Fellowship for Science and Engineering, and support
from the US National Science Foundation under grant number AST-0807690.
NR 26
TC 53
Z9 53
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 502
IS 2
BP 695
EP 703
DI 10.1051/0004-6361/200912463
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480XA
UT WOS:000268769200030
ER
PT J
AU Kainulainen, JT
Alves, JF
Beletsky, Y
Ascenso, J
Kainulainen, JM
Amorim, A
Lima, J
Marques, R
Moitinho, A
Pinhao, J
Rebordao, J
Santos, FD
AF Kainulainen, J. T.
Alves, J. F.
Beletsky, Y.
Ascenso, J.
Kainulainen, J. M.
Amorim, A.
Lima, J.
Marques, R.
Moitinho, A.
Pinhao, J.
Rebordao, J.
Santos, F. D.
TI Uncovering the kiloparsec-scale stellar ring of NGC 5128
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: dust, extinction; galaxies: individual: NGC 5128; galaxies: ISM;
galaxies: structure; infrared: galaxies
ID CENTAURUS-A; MOLECULAR GAS; WARPED DISK; DUST; PERFORMANCE; KINEMATICS;
GALAXIES; DYNAMICS; CLOUDS; NAOS
AB We reveal the stellar light emerging from the kiloparsec-scale, ring-like structure of the NGC 5128 (Centaurus A) galaxy in unprecedented detail. We use arcsecond-scale resolution near infrared images to create a "dust-free" view of the central region of the galaxy, which we then use to quantify the shape of the revealed structure. At the resolution of the data, the structure contains several hundreds of discreet, point-like or slightly elongated sources. The typical extinction-corrected surface brightness of the structure is K(S) approximate to 16.5 mag/arcsec(2), and we estimate the total near infrared luminosity of the structure to be M approximate to -21 mag. We use diffraction limited (FWHM resolution of approximate to 0.1 '', or 1.6 pc) near infrared data taken with the NACO instrument on the VLT to show that the structure decomposes into thousands of separate, mostly point-like sources. According to the tentative photometry, the most luminous sources have M(K) approximate to -12 mag, making them red supergiants or relatively low-mass star clusters. We also discuss the large-scale geometry implied by the reddening signatures of dust in our near infrared images.
C1 [Kainulainen, J. T.] Univ Helsinki, FIN-00014 Helsinki, Finland.
[Kainulainen, J. T.] TKK Metsahovi Radio Observ, Kylmala 02540, Finland.
[Alves, J. F.] Centro Astron Hispano, Calar Alto Observ, Almeria 04004, Spain.
[Beletsky, Y.] European So Observ, Santiago 19, Chile.
[Ascenso, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kainulainen, J. M.] TKK, Dept Radio Sci & Engn, Helsinki 02015, Finland.
[Amorim, A.; Lima, J.; Moitinho, A.; Santos, F. D.] Univ Lisbon, Fac Ciencias, SIM IDL, P-1749016 Lisbon, Portugal.
[Marques, R.; Pinhao, J.] Univ Coimbra, Dept Phys, LIP Coimbra, P-3004516 Coimbra, Portugal.
[Rebordao, J.] INETI, P-2720866 Amadora, Portugal.
RP Kainulainen, JT (reprint author), Univ Helsinki, POB 14, FIN-00014 Helsinki, Finland.
EM jtkainul@mpia-hd.mpg.de
RI LNEG, Producao Cientifica/D-2212-2012; Amorim, Antonio/C-8460-2013;
Santos, Filipe/M-7709-2013; Rebordao, Jose Manuel/M-3269-2013; Moitinho
de Almeida, Andre/L-1624-2015;
OI Marques, Rui/0000-0003-3549-8198; Amorim, Antonio/0000-0003-0638-2321;
Santos, Filipe/0000-0001-7316-1479; Rebordao, Jose
Manuel/0000-0002-7418-0345; Moitinho de Almeida,
Andre/0000-0003-0822-5995; Alves, Joao/0000-0002-4355-0921
NR 23
TC 11
Z9 11
U1 0
U2 5
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2009
VL 502
IS 2
BP L5
EP U16
DI 10.1051/0004-6361/200912624
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480XA
UT WOS:000268769200002
ER
PT J
AU Cowan, NB
Agol, E
Meadows, VS
Robinson, T
Livengood, TA
Deming, D
Lisse, CM
A'Hearn, MF
Wellnitz, DD
Seager, S
Charbonneau, D
AF Cowan, Nicolas B.
Agol, Eric
Meadows, Victoria S.
Robinson, Tyler
Livengood, Timothy A.
Deming, Drake
Lisse, Carey M.
A'Hearn, Michael F.
Wellnitz, Dennis D.
Seager, Sara
Charbonneau, David
CA EPOXI Team
TI ALIEN MAPS OF AN OCEAN-BEARING WORLD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planetary systems
ID DISK-AVERAGED SPECTRA; EXTRASOLAR PLANETS; EARTHSHINE OBSERVATIONS; HD
189733B; ALBEDO; DETECTABILITY; REFLECTANCE; BRIGHTNESS; MISSION
AB When Earth-mass extrasolar planets first become detectable, one challenge will be to determine which of these worlds harbor liquid water, a widely used criterion for habitability. Some of the first observations of these planets will consist of disc-averaged, time-resolved broadband photometry. To simulate such data, the Deep Impact spacecraft obtained light curves of Earth at seven wavebands spanning 300-1000 nm as part of the EPOXI mission of opportunity. In this paper, we analyze disc-integrated light curves, treating Earth as if it were an exoplanet, to determine if we can detect the presence of oceans and continents. We present two observations each spanning 1 day, taken at gibbous phases of 57 degrees and 77 degrees, respectively. As expected, the time-averaged spectrum of Earth is blue at short wavelengths due to Rayleigh scattering, and gray redward of 600 nm due to reflective clouds. The rotation of the planet leads to diurnal albedo variations of 15%-30%, with the largest relative changes occurring at the reddest wavelengths. To characterize these variations in an unbiased manner, we carry out a principal component analysis of the multi-band light curves; this analysis reveals that 98% of the diurnal color changes of Earth are due to only two dominant eigencolors. We use the time variations of these two eigencolors to construct longitudinal maps of the Earth, treating it as a non-uniform Lambert sphere. We find that the spectral and spatial distributions of the eigencolors correspond to cloud-free continents and oceans despite the fact that our observations were taken on days with typical cloud cover. We also find that the near-infrared wavebands are particularly useful in distinguishing between land and water. Based on this experiment, we conclude that it should be possible to infer the existence of water oceans on exoplanets with time-resolved broadband observations taken by a large space-based coronagraphic telescope.
C1 [Cowan, Nicolas B.; Agol, Eric; Meadows, Victoria S.; Robinson, Tyler] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Cowan, Nicolas B.; Agol, Eric; Meadows, Victoria S.; Robinson, Tyler] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Livengood, Timothy A.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Livengood, Timothy A.; A'Hearn, Michael F.; Wellnitz, Dennis D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, SD SRE, Laurel, MD 20723 USA.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA.
[Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cowan, NB (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM cowan@astro.washington.edu
RI Wellnitz, Dennis/B-4080-2012; Livengood, Timothy/C-8512-2012; Agol,
Eric/B-8775-2013; Lisse, Carey/B-7772-2016
OI Charbonneau, David/0000-0002-9003-484X; Agol, Eric/0000-0002-0802-9145;
Lisse, Carey/0000-0002-9548-1526
NR 39
TC 61
Z9 61
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 915
EP 923
DI 10.1088/0004-637X/700/2/915
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100002
ER
PT J
AU Kallivayalil, N
Besla, G
Sanderson, R
Alcock, C
AF Kallivayalil, Nitya
Besla, Gurtina
Sanderson, Robyn
Alcock, Charles
TI REVISITING THE ROLE OF M31 IN THE DYNAMICAL HISTORY OF THE MAGELLANIC
CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: interactions; galaxies: kinematics and
dynamics; Local Group; Magellanic Clouds
ID PERTURBATIVE LEAST ACTION; COLD DARK-MATTER; LOCAL GROUP; MILKY-WAY;
PROPER MOTION; ANDROMEDA GALAXY; DWARF SATELLITES; TIMING ARGUMENT;
MASS; DISTANCE
AB We study the dynamics of the Magellanic Clouds in a model for the Local Group whose mass is constrained using the timing argument/two-body limit of the action principle. The goal is to evaluate the role of M31 in generating the high angular momentum orbit of the Clouds, a puzzle that has only been exacerbated by the latest Hubble Space Telescope proper motion measurements. We study the effects of varying the total Local Group mass, the relative mass of the Milky Way (MW) and M31, the proper motion of M31, and the proper motion of the Large Magellanic Cloud (LMC) on this problem. Over a large part of this parameter space, we find that tides from M31 are insignificant. For a range of LMC proper motions approximately 3 sigma higher than the mean and total Local Group mass > 3.5 x 10(12) M(circle dot), M31 can provide a significant torque to the LMC orbit. However, if the LMC is bound to the MW, then M31 is found to have negligible effect on its motion, and the origin of the high angular momentum of the system remains a puzzle. Finally, we use the timing argument to calculate the total mass of the MW-LMC system based on the assumption that they are encountering each other for the first time, their previous perigalacticon being a Hubble time ago, obtaining M(MW) + M(LMC) = (8.7 +/- 0.8) x 10(11) M(circle dot).
C1 [Kallivayalil, Nitya; Sanderson, Robyn] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Besla, Gurtina; Alcock, Charles] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kallivayalil, N (reprint author), MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA.
EM nitya@mit.edu
OI Sanderson, Robyn/0000-0003-3939-3297
NR 53
TC 15
Z9 15
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 924
EP 930
DI 10.1088/0004-637X/700/2/924
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100003
ER
PT J
AU Bode, P
Ostriker, JP
Vikhlinin, A
AF Bode, Paul
Ostriker, Jeremiah P.
Vikhlinin, Alexey
TI EXPLORING THE ENERGETICS OF INTRACLUSTER GAS WITH A SIMPLE AND ACCURATE
MODEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE cosmology: theory; galaxies: clusters: general; intergalactic medium;
X-rays: galaxies: clusters
ID X-RAY-CLUSTERS; IA SUPERNOVA RATE; ATACAMA-COSMOLOGY-TELESCOPE; REDSHIFT
GALAXY CLUSTERS; SCALING RELATIONS; BARYON FRACTION; STAR-FORMATION; AGN
FEEDBACK; XMM-NEWTON; HYDRODYNAMICAL SIMULATIONS
AB The state of the hot gas in clusters of galaxies is investigated with a set of model clusters, created by assuming a polytropic equation of state (Gamma = 1.2) and hydrostatic equilibrium inside gravitational potential wells drawn from a dark matter (DM) simulation. Star formation, energy input, and nonthermal pressure support are included. To match the gas fractions seen in nonradiative hydrodynamical simulations, roughly 5% of the binding energy of the DM must be transferred to the gas during cluster formation; the presence of nonthermal pressure support increases this value. In order to match X-ray observations, scale-free behavior must be broken. This can be due to either variation of the efficiency of star formation with cluster mass M(500), or the input of additional energy proportional to the formed stellar mass M(F). These two processes have similar effects on X-ray scalings. If 9% of the gas is converted into stars, independent of cluster mass, then feedback energy input of 1.2 x 10(-5) M(F)c(2) (or similar to 1.0 keV per particle) is required to match observed clusters. Alternatively, if the stellar mass fraction varies as alpha M(500)(-0.26) then a lower feedback of 4 x 10(-6) M(F)c(2) is needed, and if the stellar fraction varies as steeply as alpha M(500)(-0.49) then no additional feedback is necessary. The model clusters reproduce the observed trends of gas temperature and gas mass fraction with cluster mass, as well as observed entropy and pressure profiles; thus they provide a calibrated basis with which to interpret upcoming Sunyaev-Zeldovich surveys. One consequence of the increased gas energy is that the baryon fraction inside the virial radius is less than or similar to 90% of the cosmic mean, even for the most massive clusters.
C1 [Bode, Paul; Ostriker, Jeremiah P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bode, P (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
EM bode@astro.princeton.edu; ostriker@princeton.edu;
avikhlinin@cfa.harvard.edu
NR 101
TC 50
Z9 50
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 989
EP 999
DI 10.1088/0004-637X/700/2/989
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100012
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Bautista, M
Beilicke, M
Benbow, W
Bottcher, M
Bradbury, SM
Bugaev, V
Butt, Y
Butt, Y
Byrum, K
Cannon, A
Cesarini, A
Chow, YC
Ciupik, L
Cogan, P
Colin, P
Cui, W
Daniel, M
Dickherber, R
Ergin, T
Falcone, A
Fegan, SJ
Finley, JP
Fortin, P
Fortson, L
Furniss, A
Gall, D
Gillanders, GH
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Hays, E
Holder, J
Horan, D
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kieda, D
Kildea, J
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McCann, A
McCutcheon, M
Millis, J
Moriarty, P
Mukherjee, R
Nagai, T
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Perkins, JS
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Schroedter, M
Sembroski, GH
Smith, AW
Steele, D
Stroh, M
Swordy, S
Theiling, M
Toner, JA
Varlotta, A
Vassiliev, VV
Wagner, RG
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
White, RJ
Williams, DA
Wissel, S
Wood, M
Zitzer, B
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Bautista, M.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bradbury, S. M.
Bugaev, V.
Butt, Y.
Butt, Y.
Byrum, K.
Cannon, A.
Cesarini, A.
Chow, Y. C.
Ciupik, L.
Cogan, P.
Colin, P.
Cui, W.
Daniel, M.
Dickherber, R.
Ergin, T.
Falcone, A.
Fegan, S. J.
Finley, J. P.
Fortin, P.
Fortson, L.
Furniss, A.
Gall, D.
Gillanders, G. H.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Hays, E.
Holder, J.
Horan, D.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kieda, D.
Kildea, J.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McCann, A.
McCutcheon, M.
Millis, J.
Moriarty, P.
Mukherjee, R.
Nagai, T.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Perkins, J. S.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. Joachim
Schroedter, M.
Sembroski, G. H.
Smith, A. W.
Steele, D.
Stroh, M.
Swordy, S.
Theiling, M.
Toner, J. A.
Varlotta, A.
Vassiliev, V. V.
Wagner, R. G.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
White, R. J.
Williams, D. A.
Wissel, S.
Wood, M.
Zitzer, B.
TI MULTIWAVELENGTH OBSERVATIONS OF LS I+61 degrees 303 WITH VERITAS, SWIFT,
AND RXTE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gamma rays: observations; X-rays: binaries
ID X-RAY BINARY; ENERGY GAMMA-RAYS; MICROQUASAR LS-I+61-303;
TIMING-EXPLORER; RADIO; TELESCOPE; SPECTRUM; LSI+61-DEGREES-303;
+61-DEGREES-303; LS-I-+61-303
AB We present results from a long-term monitoring campaign on the TeV binary LSI +61 degrees 303 with VERITAS at energies above 500 GeV, and in the 2-10 keV hard X-ray bands with RXTE and Swift, sampling nine 26.5 day orbital cycles between 2006 September and 2008 February. The binary was observed by VERITAS to be variable, with all integrated observations resulting in a detection at the 8.8 sigma (2006/2007) and 7.3 sigma (2007/2008) significance level for emission above 500 GeV. The source was detected during active periods with flux values ranging from 5% to 20% of the Crab Nebula, varying over the course of a single orbital cycle. Additionally, the observations conducted in the 2007-2008 observing season show marginal evidence (at the 3.6 sigma significance level) for TeV emission outside the apastron passage of the compact object around the Be star. Contemporaneous hard X-ray observations with RXTE and Swift show large variability with flux values typically varying between 0.5 and 3.0 x 10(-11) erg cm(-2) s(-1) over a single orbital cycle. The contemporaneous X-ray and TeV data are examined and it is shown that the TeV sampling is not dense enough to detect a correlation between the two bands.
C1 [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Arlen, T.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Kildea, J.; Perkins, J. S.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Bradbury, S. M.; Daniel, M.; Rose, H. Joachim; White, R. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Butt, Y.; Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Colin, P.; Hui, C. M.; Kildea, J.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Falcone, A.; Stroh, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Fortin, P.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Humensky, T. B.; Swordy, S.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
RP Acciari, VA (reprint author), Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland.
EM awsmith@hep.anl.gov
RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010;
OI Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910;
Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794
FU U. S. Department of Energy; U. S. National Science Foundation;
Smithsonian Institution; NSERC in Canada; Science Foundation Ireland;
PPARC; U. S. Department of Energy Office of Science laboratory
[DE-AC02-06CH11357]
FX The submitted manuscript has been created by UChicago Argonne, LLC,
Operator of Argonne National Laboratory ("Argonne"). Argonne, a U. S.
Department of Energy Office of Science laboratory, is operated under
Contract No. DE-AC02-06CH11357. The U. S. Government retains for itself,
and others acting on its behalf, a paid-up nonexclusive, irrevocable
worldwide license in said article to reproduce, prepare derivative
works, distribute copies to the public, and perform publicly and display
publicly, by or on behalf of the Government.
NR 48
TC 23
Z9 23
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1034
EP 1041
DI 10.1088/0004-637X/700/2/1034
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100017
ER
PT J
AU Hicken, M
Wood-Vasey, WM
Blondin, S
Challis, P
Jha, S
Kelly, PL
Rest, A
Kirshner, RP
AF Hicken, Malcolm
Wood-Vasey, W. Michael
Blondin, Stephane
Challis, Peter
Jha, Saurabh
Kelly, Patrick L.
Rest, Armin
Kirshner, Robert P.
TI IMPROVED DARK ENERGY CONSTRAINTS FROM similar to 100 NEW CfA SUPERNOVA
TYPE Ia LIGHT CURVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: dark energy; supernovae: general
ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; LEGACY SURVEY;
GALAXIES; EXTINCTION; EVOLUTION; SPECTROSCOPY; LUMINOSITY; CONSTANT;
OMEGA(LAMBDA)
AB We combine the CfA3 supernovae Type Ia (SN Ia) sample with samples from the literature to calculate improved constraints on the dark energy equation of state parameter, w. The CfA3 sample is added to the Union set of Kowalski et al. to form the Constitution set and, combined with a BAO prior, produces 1 + w = 0.013(-0.068)(+0.066) (0.11 syst), consistent with the cosmological constant. The CfA3 addition makes the cosmologically useful sample of nearby SN Ia between 2.6 and 2.9 times larger than before, reducing the statistical uncertainty to the point where systematics play the largest role. We use four light-curve fitters to test for systematic differences: SALT, SALT2, MLCS2k2 (R(V) = 3.1), and MLCS2k2 (R(V) = 1.7). SALT produces high-redshift Hubble residuals with systematic trends versus color and larger scatter than MLCS2k2. MLCS2k2 overestimates the intrinsic luminosity of SN Ia with 0.7 < Delta < 1.2. MLCS2k2 with R(V) = 3.1 overestimates host-galaxy extinction while R(V) approximate to 1.7 does not. Our investigation is consistent with no Hubble bubble. We also find that, after light-curve correction, SN Ia in Scd/Sd/Irr hosts are intrinsically fainter than those in E/S0 hosts by 2 sigma, suggesting that they may come from different populations. We also find that SN Ia in Scd/Sd/Irr hosts have low scatter (0.1 mag) and reddening. Current systematic errors can be reduced by improving SN Ia photometric accuracy, by including the CfA3 sample to retrain light-curve fitters, by combining optical SN Ia photometry with near-infrared photometry to understand host-galaxy extinction, and by determining if different environments give rise to different intrinsic SN Ia luminosity after correction for light-curve shape and color.
C1 [Hicken, Malcolm; Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hicken, Malcolm; Rest, Armin] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Blondin, Stephane] European So Observ, D-85748 Garching, Germany.
[Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kelly, Patrick L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Rest, Armin] Cerro Tololo Inter Amer Observ CTIO, La Serena, Chile.
RP Hicken, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM kirshner@cfa.harvard.edu
FU NSF [AST0606772]; Goldberg Fellowship Program
FX This work has been supported, in part, by NSF grant AST0606772 to
Harvard University. A. R. thanks the Goldberg Fellowship Program for its
support.
NR 58
TC 544
Z9 546
U1 0
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1097
EP 1140
DI 10.1088/0004-637X/700/2/1097
PG 44
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100024
ER
PT J
AU de Val-Borro, M
Karovska, M
Sasselov, D
AF de Val-Borro, M.
Karovska, M.
Sasselov, D.
TI NUMERICAL SIMULATIONS OF WIND ACCRETION IN SYMBIOTIC BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: symbiotic; hydrodynamics; methods:
numerical; stars: mass loss; stars: winds, outflows
ID GIANT-BRANCH STARS; PLANETARY-NEBULAE; R-AQUARII; AGB STAR; DUST; DISC;
FLOW; EVOLUTION; SYSTEM; CODE
AB About half of the binary systems are close enough to each other for mass to be exchanged between them at some point in their evolution, yet the accretion mechanism in wind accreting binaries is not well understood. We study the dynamical effects of gravitational focusing by a binary companion on winds from late-type stars. In particular, we investigate the mass transfer and formation of accretion disks around the secondary in detached systems consisting of an asymptotic giant branch (AGB) mass-losing star and an accreting companion. The presence of mass outflows is studied as a function of mass-loss rate, wind temperature, and binary orbital parameters. A two-dimensional hydrodynamical model is used to study the stability of mass transfer in wind accreting symbiotic binary systems. In our simulations we use an adiabatic equation of state and a modified version of the isothermal approximation, where the temperature depends on the distance from the mass losing star and its companion. The code uses a block-structured adaptive mesh refinement method that allows us to have high resolution at the position of the secondary and resolve the formation of bow shocks and accretion disks. We explore the accretion flow between the components and formation of accretion disks for a range of orbital separations and wind parameters. Our results show the formation of stream flow between the stars and accretion disks of various sizes for certain orbital configurations. For a typical slow and massive wind from an AGB star the flow pattern is similar to a Roche lobe overflow with accretion rates of 10% of the mass loss from the primary. Stable disks with exponentially decreasing density profiles and masses of the order 10(-4) solar masses are formed when wind acceleration occurs at several stellar radii. The disks are geometrically thin with eccentric streamlines and close to Keplerian velocity profiles. The formation of tidal streams and accretion disks is found to be weakly dependent on the mass loss from the AGB star. Our simulations of gravitationally focused wind accretion in symbiotic binaries show the formation of stream flows and enhanced accretion rates onto the compact component. We conclude that mass transfer through a focused wind is an important mechanism in wind accreting interacting binaries and can have a significant impact on the evolution of the binary itself and the individual components.
C1 [de Val-Borro, M.; Karovska, M.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[de Val-Borro, M.] Stockholm Univ, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden.
RP de Val-Borro, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI de Val-Borro, Miguel/H-1319-2013
OI de Val-Borro, Miguel/0000-0002-0455-9384
NR 56
TC 38
Z9 38
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1148
EP 1160
DI 10.1088/0004-637X/700/2/1148
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100026
ER
PT J
AU Zhu, L
Zhang, SN
Tang, SM
AF Zhu, Ling
Zhang, Shuang Nan
Tang, Sumin
TI EVIDENCE FOR AN INTERMEDIATE LINE REGION IN ACTIVE GALACTIC NUCLEI's
INNER TORUS REGION AND ITS EVOLUTION FROM NARROW TO BROAD LINE SEYFERT I
GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article; Proceedings Paper
CT Black Hole Workshop
CY APR 26-28, 2008
CL Shanghai Astron Observ, Shanghai, PEOPLES R CHINA
HO Shanghai Astron Observ
DE galaxies: active; galaxies: nuclei; galaxies: structure; Galaxy:
evolution; line: profiles; quasars: emission lines
ID BLACK-HOLE MASS; DIGITAL SKY SURVEY; BH-SIGMA RELATION; AGN DUSTY TORI;
EMISSION-LINE; VELOCITY DISPERSION; H-BETA; REVERBERATION MEASUREMENTS;
MICROLENSING PROBES; UNIFIED SCHEMES
AB A two-component model for the broad-line region (BLR) of active galactic nuclei (AGNs) has been suggested for many years but not widely accepted. This model indicates that the broad line can be described with the superposition of two Gaussian components (very broad Gaussian component and intermediate Gaussian component (IMGC)) which are from two physically distinct regions, i.e., very broad line region (VBLR) and intermediate line region. We select a Sloan Digital Sky Survey sample to further confirm this model and give a detailed analysis of the geometry, density, and evolution of these two regions. The microlensing result of the BLR in J1131-1231 and some unexplained phenomena in reverberation mapping (RM) experiment provide supportive evidence for this model. Our results indicate that the radius obtained from the emission line RM normally corresponds to the radius of the VBLR, and the existence of the IMGC may affect the measurement of the black hole masses in AGNs. The deviation of NLS1s from the M-sigma relation and the type II AGN fraction as a function of luminosity can be explained in this model in a coherent way. The evolution of the two emission regions may be related to the evolutionary stages of the BLRs of AGNs from NLS1s to BLS1s. Based on the results presented here, a unified picture of the hierarchical evolution of a black hole, a dust torus, and a galaxy is proposed.
C1 [Zhu, Ling; Zhang, Shuang Nan] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Zhu, Ling; Zhang, Shuang Nan] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China.
[Zhang, Shuang Nan] Chinese Acad Sci, Key Lab Particle Astrophys, Inst High Energy Phys, Beijing 100049, Peoples R China.
[Zhang, Shuang Nan] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Tang, Sumin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zhang, SN (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
EM zhul04@mails.tsinghua.edu.cn; zhangsn@tsinghua.edu.cn
NR 75
TC 34
Z9 34
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1173
EP 1189
DI 10.1088/0004-637X/700/2/1173
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100028
ER
PT J
AU Desai, V
Soifer, BT
Dey, A
Le Floc'h, E
Armus, L
Brand, K
Brown, MJI
Brodwin, M
Jannuzi, BT
Houck, JR
Weedman, DW
Ashby, MLN
Gonzalez, A
Huang, J
Smith, HA
Teplitz, H
Willner, SP
Melbourne, J
AF Desai, Vandana
Soifer, B. T.
Dey, Arjun
Le Floc'h, Emeric
Armus, Lee
Brand, Kate
Brown, Michael J. I.
Brodwin, Mark
Jannuzi, Buell T.
Houck, James R.
Weedman, Daniel W.
Ashby, Matthew L. N.
Gonzalez, Anthony
Huang, Jiasheng
Smith, Howard A.
Teplitz, Harry
Willner, Steve P.
Melbourne, Jason
TI STRONG POLYCYCLIC AROMATIC HYDROCARBON EMISSION FROM z approximate to 2
ULIRGs
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies:
starburst; infrared: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; DUST-OBSCURED
GALAXIES; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATES; IRAC SHALLOW
SURVEY; ARRAY CAMERA IRAC; MU-M OBSERVATIONS; HIGH-REDSHIFT; MIDINFRARED
SPECTROSCOPY
AB Using the Infrared Spectrograph on board the Spitzer Space Telescope, we present low-resolution (64 < lambda/delta lambda < 124), mid-infrared (20-38 mu m) spectra of 23 high-redshift ULIRGs detected in the Bootes field of the NOAO Deep Wide-Field Survey. All of the sources were selected to have (1) f(v)(24 mu m) > 0.5mJy; (2) R-[24] > 14 Vega mag; and (3) a prominent rest frame 1.6 mu m stellar photospheric feature redshifted into Spitzer's 3-8 mu m IRAC bands. Of these, 20 show emission from polycyclic aromatic hydrocarbons (PAHs), usually interpreted as signatures of star formation. The PAH features indicate redshifts in the range 1.5 < z < 3.0, with a mean of < z > = 1.96 and a dispersion of 0.30. Based on local templates, these sources have extremely large infrared luminosities, comparable to that of submillimeter galaxies. Our results confirm previous indications that the rest-frame 1.6 mu m stellar bump can be efficiently used to select highly obscured star-forming galaxies at z approximate to 2, and that the fraction of starburst-dominated ULIRGs increases to faint 24 mu m flux densities. Using local templates, we find that the observed narrow redshift distribution is due to the fact that the 24 mu m detectability of PAH-rich sources peaks sharply at z = 1.9. We can analogously use observed spectral energy distributions to explain the broader redshift distribution of Spitzer-detected ULIRGs that are dominated by an active galactic nucleus (AGN). Finally, we conclude that z approximate to 2 sources with a detectable 1.6 mu m stellar opacity feature lack sufficient AGN emission to veil the 7.7 mu m PAH band.
C1 [Desai, Vandana; Soifer, B. T.; Melbourne, Jason] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Desai, Vandana; Soifer, B. T.; Armus, Lee; Teplitz, Harry] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Dey, Arjun; Brand, Kate; Brodwin, Mark; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Le Floc'h, Emeric] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Brand, Kate] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Brodwin, Mark; Ashby, Matthew L. N.; Huang, Jiasheng; Smith, Howard A.; Willner, Steve P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Houck, James R.; Weedman, Daniel W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Gonzalez, Anthony] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
RP Desai, V (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
NR 68
TC 40
Z9 41
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1190
EP 1204
DI 10.1088/0004-637X/700/2/1190
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100029
ER
PT J
AU Torres, G
Claret, A
Young, PA
AF Torres, Guillermo
Claret, Antonio
Young, Patrick A.
TI BINARY ORBIT, PHYSICAL PROPERTIES, AND EVOLUTIONARY STATE OF CAPELLA
(alpha AURIGAE)
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE binaries: general; binaries: spectroscopic; stars: abundances; stars:
evolution; stars: fundamental parameters; stars: individual (Capella)
ID SPECKLE INTERFEROMETRIC MEASUREMENTS; LINED SPECTROSCOPIC BINARIES;
CHROMOSPHERICALLY ACTIVE STARS; PREDICTIVE STELLAR EVOLUTION;
RADIAL-VELOCITY MEASUREMENTS; DETACHED ECLIPSING BINARIES;
LIMB-DARKENING COEFFICIENTS; PEAK 4-M TELESCOPE; RED CLUMP GIANTS;
X-RAY-EMISSION
AB We report extensive radial velocity measurements of the two giant components of the detached, 104 day period binary system of Capella. Our highly accurate three-dimensional orbital solution based on all existing spectroscopic and astrometric observations including our own yields much improved masses for the primary and secondary of 2.466 +/- 0.018 M-circle dot and 2.443 +/- 0.013 M-circle dot, with relative errors of only 0.7% and 0.5%, respectively. The mass ratio is considerably closer to unity than previously believed, which has an impact on assessing the evolutionary state of the system. Improved values are presented also for the radii (11.87 +/- 0.56 R-circle dot and 8.75 +/- 0.32 R-circle dot), effective temperatures (4920 +/- 70 K and 5680 +/- 70 K), and luminosities (79.5 +/- 4.8 L-circle dot and 72.1 +/- 3.6 L-circle dot). The distance is determined to be 13.042 +/- 0.028 pc, based on the accurate orbital parallax. The projected rotational velocities and individual rotation periods are also known. Capella is unique among evolved stars in that, in addition to all of the above, the chemical composition is known as well. This includes the overall metallicity [m/H], the carbon isotope ratio C-12/C-13 for the primary, and the lithium abundance and C-to-N ratios for both components. We present new or revised values for some of these. The latter three quantities are sensitive diagnostics of evolution, and change drastically for giants as a result of the deepening of the convective envelope during the first dredge-up. The secondary is crossing the Hertzprung gap, while the primary is believed to be in the longer-lived core helium-burning phase. Previous studies using only the masses, temperatures, and luminosities have found good agreement with stellar evolution models placing the primary in the clump. Here, we compare all of the constraints simultaneously against three sets of current models. We find that they are unable to match all of the observations for both components at the same time, and at a single age, for any evolutionary state of the primary. This shows the great importance of chemical information for assessing the evolutionary state of giant stars. A comparison with models of tidal evolution yields similarly disappointing results, when tested against the fact that the orbit is circular, the primary is rotating synchronously, the secondary similar to 12 times faster than synchronous, and the spin axes are apparently aligned with the axis of the orbit. When confronted in detail, our understanding of the advanced stages of stellar evolution is thus still very incomplete.
C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Young, Patrick A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gtorres@cfa.harvard.edu; claret@iaa.es; patrick.young.1@asu.edu
NR 207
TC 28
Z9 28
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 AUG 1
PY 2009
VL 700
IS 2
BP 1349
EP 1381
DI 10.1088/0004-637X/700/2/1349
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100038
ER
PT J
AU Randall, SW
Jones, C
Markevitch, M
Blanton, EL
Nulsen, PEJ
Forman, WR
AF Randall, S. W.
Jones, C.
Markevitch, M.
Blanton, E. L.
Nulsen, P. E. J.
Forman, W. R.
TI GAS SLOSHING AND BUBBLES IN THE GALAXY GROUP NGC 5098
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (RGH80, NSCS
J132014+330824) galaxies: individual (NGC5098); X-rays: galaxies
ID FLOW CLUSTER ABELL-2052; ACTIVE GALACTIC NUCLEI; X-RAY CAVITIES; COLD
FRONTS; CHANDRA OBSERVATION; XMM-NEWTON; SKY SURVEY; HOT GAS; SHOCK;
CORE
AB We present results from Chandra observations of the galaxy pair and associated galaxy group NGC 5098, and find evidence for both gas sloshing and active galactic nucleus (AGN) heating. The X-ray brightness images show diffuse emission with a spiral structure, centered on NGC 5098a, and a sharp edge in the diffuse emission surrounding much of the galaxy at about 30 kpc. The spiral structure in the X-ray surface brightness and temperature maps, the offset between the peak of the cool gas and the central AGN, and the structure of the cold front edges all suggest gas sloshing in the core. The most likely perturber is the nearby galaxy NGC 5098b, which has been stripped of its gaseous atmosphere. Detailed images of the core reveal several X-ray cavities, two of which, just north and southeast of the central AGN, correlate with radio emission and have bright X-ray rims, similar to buoyant bubbles seen in the intracluster medium of other systems. We estimate the pressures in the bubbles and rims and show that they are roughly equal, consistent with these being young features, as suggested by their close proximity to the central AGN. We assume that the other X-ray cavities in the core, which show no correlation with existing radio observations, are ghost cavities from previous AGN outbursts. An estimate of the mechanical energy required to inflate the cavities indicates that it is sufficient to offset radiative cooling of the gas for 15 Myr. Therefore, for a typical cycle time of 10(7) yr, the central AGN energy output is enough to balance cooling over long timescales.
C1 [Randall, S. W.; Jones, C.; Markevitch, M.; Nulsen, P. E. J.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
RP Randall, SW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM srandall@cfa.harvard.edu; cjf@cfa.harvard.edu;
mmarkevitch@cfa.harvard.edu; eblanton@bu.edu; wrf@cfa.harvard.edu
RI Blanton, Elizabeth/H-4501-2014;
OI Randall, Scott/0000-0002-3984-4337; Nulsen, Paul/0000-0003-0297-4493
FU Chandra X-ray Center; NASA [NAS8-03060]; Smithsonian Institution
FX The financial support for this work was partially provided for by the
Chandra X-ray Center through NASA contract NAS8-03060 and the
Smithsonian Institution. We thank the anonymous referee for useful
comments.
NR 43
TC 25
Z9 25
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1404
EP 1414
DI 10.1088/0004-637X/700/2/1404
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100041
ER
PT J
AU Johns-Krull, CM
Greene, TP
Doppmann, GW
Covey, KR
AF Johns-Krull, Christopher M.
Greene, Thomas P.
Doppmann, Greg W.
Covey, Kevin R.
TI FIRST MAGNETIC FIELD DETECTION ON A CLASS I PROTOSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: individual (WL 17); stars: pre-main
sequence
ID T-TAURI STARS; MAIN-SEQUENCE STARS; AURIGA MOLECULAR CLOUD; YOUNG
STELLAR OBJECTS; NEAR-INFRARED SPECTRA; RHO-OPHIUCHI CLOUD;
MAGNETOSPHERIC ACCRETION; BP TAURI; ENERGY-DISTRIBUTIONS; EVOLUTIONARY
STATUS
AB Strong stellar magnetic fields are believed to truncate the inner accretion disks around young stars, redirecting the accreting material to the high latitude regions of the stellar surface. In the past few years, observations of strong stellar fields on T Tauri stars with field strengths in general agreement with the predictions of magnetospheric accretion theory have bolstered this picture. Currently, nothing is known about the magnetic field properties of younger, more embedded Class I young stellar objects. It is believed that protostars accrete much of their final mass during the Class I phase, but the physics governing this process remains poorly understood. Here, we use high-resolution near-infrared spectra obtained with NIRSPEC on Keck and with Phoenix on Gemini South to measure the magnetic field properties of the Class I protostar WL 17. We find clear signatures of a strong stellar magnetic field. Analysis of this data suggests a surface average field strength of 2.9 +/- 0.43 kG on WL 17. We present our field measurements and discuss how they fit with the general model of magnetospheric accretion in young stars.
C1 [Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Doppmann, Greg W.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Covey, Kevin R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Johns-Krull, CM (reprint author), Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
EM cmj@rice.edu; thomas.p.greene@nasa.gov; gdoppmann@noao.edu;
kcovey@cfa.harvard.edu
OI Covey, Kevin/0000-0001-6914-7797
FU NASA Origins of Solar Systems program [NAG5-13103, NNG06GD85G]; Spitzer
Space Telescope Fellowship Program; Jet Propulsion Laboratory;
California Institute of Technology
FX We are pleased to acknowledge numerous, stimulating discussions with J.
Valenti on all aspects of the work reported here. We also acknowledge
many useful comments and suggestions from an anonymous referee. C. M.
J.-K. acknowledge partial support for this research from the NASA
Origins of Solar Systems program through grant numbers NAG5-13103 and
NNG06GD85G made to Rice University. T. P. G. acknowledges support from
NASA's Origins of Solar Systems program via WBS 811073.02.07.01.89. K.
R. C. acknowledges support for this work by NASA through the Spitzer
Space Telescope Fellowship Program, through a contract issued by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. This work made use of the SIMBAD reference database,
the NASA Astrophysics Data System, and VALD line database.
NR 83
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1440
EP 1448
DI 10.1088/0004-637X/700/2/1440
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100044
ER
PT J
AU Andrews, SM
Wilner, DJ
Hughes, AM
Qi, CH
Dullemond, CP
AF Andrews, Sean M.
Wilner, D. J.
Hughes, A. M.
Qi, Chunhua
Dullemond, C. P.
TI PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE accretion, accretion disks; circumstellar matter; planetary systems:
protoplanetary disks; solar system: formation; stars: pre-main sequence
ID T-TAURI STARS; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS;
MAIN-SEQUENCE EVOLUTION; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS;
MILLIMETER CONTINUUM OBSERVATIONS; GIANT PLANET FORMATION; KUIPER-BELT
OBJECTS; SPITZER C2D SURVEY; CIRCUMSTELLAR DISKS
AB We present the results of a high angular resolution (0 ''.3 approximate to 40 AU) Submillimeter Array survey of the 345 GHz (870 mu m) thermal continuum emission from nine of the brightest, and therefore most massive, circumstellar disks in the similar to 1 Myr-old Ophiuchus star-forming region. Using two-dimensional radiative transfer calculations, we simultaneously fit the observed continuum visibilities and broadband spectral energy distribution for each disk with a parametric structure model. Compared to previous millimeter studies, this survey includes significant upgrades in modeling, data quality, and angular resolution that provide improved constraints on key structure parameters, particularly those that characterize the spatial distribution of mass in the disks. In the context of a surface density profile motivated by similarity solutions for viscous accretion disks, Sigma proportional to (R/R(c))(-gamma) exp [-(R/R(c))(2-gamma)], the best-fit models for the sample disks have characteristic radii R(c) approximate to 20-200 AU, high disk masses M(d) approximate to 0.005-0.14 M(circle dot) (a sample selection bias), and a narrow range of radial Sigma gradients (gamma approximate to 0.4-1.0) around a median gamma = 0.9. These density structures are used in conjunction with accretion rate estimates from the literature to help characterize the viscous evolution of the disk material. Using the standard prescription for disk viscosities, those combined constraints indicate that alpha approximate to 0.0005-0.08. Three of the sample disks show large (R approximate to 20-40 AU) central cavities in their continuum emission morphologies, marking extensive zones where dust has been physically removed and/or has significantly diminished opacities. Based on the current requirements of planet formation models, these emission cavities and the structure constraints for the sample as a whole suggest that these young disks may eventually produce planetary systems, and have perhaps already started.
C1 [Andrews, Sean M.; Wilner, D. J.; Hughes, A. M.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dullemond, C. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sandrews@cfa.harvard.edu; dwilner@cfa.harvard.edu;
mhughes@cfa.harvard.edu; cqi@cfa.harvard.edu; dullemon@mpia.de
OI Dullemond, Cornelis/0000-0002-7078-5910
NR 165
TC 261
Z9 261
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1502
EP 1523
DI 10.1088/0004-637X/700/2/1502
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100049
ER
PT J
AU Myers, PC
AF Myers, Philip C.
TI FILAMENTARY STRUCTURE OF STAR-FORMING COMPLEXES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; stars: formation
ID LARGE-SCALE STRUCTURE; C2D LEGACY CLOUDS; MOLECULAR CLOUDS; DENSE CORES;
DARK CLOUD; EMBEDDED-CLUSTER; SUPERSONIC TURBULENCE; GALACTIC
DISTRIBUTION; INITIAL CONDITIONS; STELLAR GROUPS
AB The nearest young stellar groups are associated with "hubs" of column density exceeding 10(22) cm(-2), according to recent observations. These hubs radiate multiple "filaments" of parsec length, having lower column density and fewer stars. Systems with many filaments tend to have parallel filaments with similar spacing. Such "hub-filament structure" is associated with all of the nine young stellar groups within 300 pc, forming low-mass stars. Similar properties are seen in infrared dark clouds forming more massive stars. In a new model, an initial clump in a uniform medium is compressed into a self-gravitating, modulated layer. The outer layer resembles the modulated equilibrium of Schmid-Burgk with nearly parallel filaments. The filaments converge onto the compressed clump, which collapses to form stars with high efficiency. The initial medium and condensations have densities similar to those in nearby star-forming clouds and clumps. The predicted structures resemble observed hub-filament systems in their size, shape, and column density, and in the appearance of their filaments. These results suggest that HFS associated with young stellar groups may arise from compression of clumpy gas in molecular clouds.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM pmyers@cfa.harvard.edu
NR 94
TC 133
Z9 133
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1609
EP 1625
DI 10.1088/0004-637X/700/2/1609
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100056
ER
PT J
AU Marengo, M
Stapelfeldt, K
Werner, MW
Hora, JL
Fazio, GG
Schuster, MT
Carson, JC
Megeath, ST
AF Marengo, Massimo
Stapelfeldt, Karl
Werner, Michael W.
Hora, Joseph L.
Fazio, Giovanni G.
Schuster, Michael T.
Carson, Joseph C.
Megeath, S. Thomas
TI SPITZER/INFRARED ARRAY CAMERA LIMITS TO PLANETARY COMPANIONS OF
FOMALHAUT AND epsilon ERIDANI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; planetary systems; stars: individual (Fomalhaut,
epsilon Eridani)
ID SPITZER-SPACE-TELESCOPE; BROWN DWARFS; DEBRIS DISK; EXTRASOLAR PLANETS;
GIANT PLANETS; CORONAGRAPHIC SEARCH; NEARBY STARS; DUST DISK; T-DWARFS;
VEGA
AB Fomalhaut and epsilon Eridani are two young, nearby stars that possess extended debris disks whose structures suggest the presence of perturbing planetary objects. With its high sensitivity and stable point-spread function, Spitzer/Infrared Array Camera (IRAC) is uniquely capable of detecting cool, Jupiter-like planetary companions whose peak emission is predicted to occur near 4.5 mu m. We report on deep IRAC imaging of these two stars, taken at 3.6 and 4.5 mu m using subarray mode and in all four channels in wider-field full array mode. Observations acquired at two different telescope roll angles allowed faint surrounding objects to be separated from the stellar diffraction pattern. No companion candidates were detected at the reported position of Fomalhaut b with 3 sigma model-dependent mass upper limits of 3M(J) (for an age of 200 Myr). Around epsilon Eridani, we instead set a limit of 4 and less than or similar to 1M(J) (1 Gyr model age) at the inner and outer edge of the submillimeter debris ring, respectively. These results are consistent with non-detections in recent near-infrared imaging searches, and set the strongest limits to date on the presence of planets outside epsilon Eridani submillimeter ring.
C1 [Marengo, Massimo; Hora, Joseph L.; Fazio, Giovanni G.; Schuster, Michael T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Megeath, S. Thomas] Univ Toledo, Toledo, OH 43606 USA.
[Carson, Joseph C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Stapelfeldt, Karl; Werner, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mmarengo@cfa.harvard.edu
RI Stapelfeldt, Karl/D-2721-2012
FU NASA under Spitzer General Observer [30754]; Harvard-Smithsonian Center
FX We thank John Krist and James Graham for their advice on PSF
subtractions and the application of the Fortney atmosphere models to our
data set. This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA under Spitzer General Observer grants
30754 to the Harvard-Smithsonian Center for Astrophysics and to JPL.
NR 41
TC 36
Z9 36
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1647
EP 1657
DI 10.1088/0004-637X/700/2/1647
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100058
ER
PT J
AU van den Berg, M
Hong, J
Grindlay, JE
AF van den Berg, Maureen
Hong, JaeSub
Grindlay, Jonathan E.
TI ChaMPlane DEEP GALACTIC BULGE SURVEY. I. FAINT ACCRETION-DRIVEN BINARIES
IN THE LIMITING WINDOW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: bulge; novae, cataclysmic variables; surveys; X-rays: binaries
ID ALL-SKY SURVEY; X-RAY SOURCES; CATACLYSMIC VARIABLE-STARS; M-DWARFS;
CORONAE; SPECTRA; CATALOG; COUNTS; SPACE; POPULATION
AB We have carried out a deep X-ray and optical survey with Chandra and HST of low-extinction regions in the Galactic bulge. Here we present the results of a search for low-luminosity (L(X) less than or similar to 10(34) erg s(-1)) accreting binaries among the Chandra sources in the region closest to the Galactic center, at an angular offset of 1.degrees 4, that we have named the Limiting Window. Based on their blue optical colors, excess H alpha fluxes, and high X-ray-to-optical flux ratios, we identify three likely accreting binaries; these are probably white dwarfs accreting from low-mass companions (cataclysmic variables; CVs) although we cannot exclude that they are quiescent neutron-star or black-hole low-mass X-ray binaries. Distance estimates put these systems farther than greater than or similar to 2 kpc. Based on their H alpha-excess fluxes and/or high X-ray-to-optical flux ratios, we find 22 candidate accreting binaries; however, the properties of some can also be explained if they are dMe stars or active galaxies. We investigate the CV number density toward the bulge and find that the number of observed candidate CVs is consistent with or lower than the number expected for a constant CV-to-star ratio that is fixed to the local value. Our conclusions are limited by uncertainties in the extinction (for which we see a similar to 30% variation in our 6.'6 x 6.'6 field) and selection effects. The X-ray properties of two likely CVs are similar to those of the faint, hard X-ray sources in the Galactic center region that have been suggested to be (mainly) magnetic CVs. If our candidates belong to the same population, they would be the first members to be optically identified; optical or infrared identification of their Galactic center analogs would be impossible due to the higher obscuration. We speculate that all Galactic hard X-ray sources in our field can be explained by magnetic CVs.
C1 [van den Berg, Maureen; Hong, JaeSub; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van den Berg, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM maureen@head.cfa.harvard.edu
FU STScI/HST [HST-GO-10353.01]; NASA/Chandra [GO6-7088X, GO7-8090X,
GO8-9093X]; Association of Universities for Research in Astronomy, Inc
[5-26555]
FX The authors thank A. Udalski for providing a list of OGLEIII variables
in our field prior to publication. We are grateful to A. Dolphin for
help with running the DOLPHOT photometry package. Our research made use
of the Sloan Digital Sky Survey database. This work was supported in
part by STScI/HST grant HST-GO-10353.01 and NASA/Chandra grants
GO6-7088X, GO7-8090X and GO8-9093X. Results in this paper are based on
observations made with the NASA/ESA Hubble Space Telescope, obtained at
the Space Telescope Institute which is operated by the Association of
Universities for Research in Astronomy, Inc. under the NASA contract NAS
5-26555.
NR 48
TC 16
Z9 16
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1702
EP 1715
DI 10.1088/0004-637X/700/2/1702
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100065
ER
PT J
AU Wang, HJ
Shen, CC
Lin, J
AF Wang, Hongjuan
Shen, Chengcai
Lin, Jun
TI NUMERICAL EXPERIMENTS OF WAVE-LIKE PHENOMENA CAUSED BY THE DISRUPTION OF
AN UNSTABLE MAGNETIC CONFIGURATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE MHD; shock waves; Sun: coronal mass ejections; Sun: flares; Sun:
magnetic fields
ID CORONAL MASS EJECTIONS; RADIATION MAGNETOHYDRODYNAMICS CODE; 2 SPACE
DIMENSIONS; II RADIO-BURSTS; SOLAR-FLARES; ASTROPHYSICAL FLOWS; FLUX
ROPE; HYDRODYNAMIC ALGORITHMS; SOHO/EIT OBSERVATIONS; ERUPTIVE FLARES
AB The origin of the Moreton wave observed in the chromosphere and the EIT wave observed in the corona during the eruption remains an active research subject. We investigate numerically in this work the evolutionary features of the magnetic configuration that includes a current-carrying flux rope, which is used to model the filament, after the loss of equilibrium in the system takes place in a catastrophic fashion. Rapid motions of the flux rope following the catastrophe invoke the velocity vortices behind the rope, and may also invoke slow-and fast-mode shocks in front of the rope. The velocity vortices at each side of the flux rope propagate roughly horizontally away from the area where they are produced, and both shocks expand toward the flank of the flux rope. The fast shock may eventually reach the bottom boundary and produce two echoes moving back into the corona, but the slow one and the vortices totally decay somewhere in the lower corona before arriving of the bottom boundary. The interaction of the fast shock with the boundary leads to disturbance that accounts for the Moreton wave observed in Ha, and the disturbance in the corona caused by the slow shock and the velocity vortices should account for the EIT wave whose speed is about 40% that of the Moreton wave. The implication of these results to the observed correlation of the type II radio burst to the fast-and the slow-mode shocks and that of EIT waves to coronal mass ejections and flares has also been discussed.
C1 [Wang, Hongjuan; Shen, Chengcai; Lin, Jun] Chinese Acad Sci, Natl Astron Observ China, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
[Wang, Hongjuan; Shen, Chengcai] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China.
[Lin, Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wang, HJ (reprint author), Chinese Acad Sci, Natl Astron Observ China, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
RI LIN, JUN/B-9890-2017
FU Program 973 [2006CB806303]; NSFC [40636031, 10873030]; CAS [KJCX2-
YW-T04]; NASA [NNX07AL72G]
FX The authors appreciate M. Zhang very much for teaching the key
techniques of running the ZEUS- 2D code smoothly. They are also grateful
to T. G. Forbes, P. Chen, G. D. R. Attrill, M. J. Wills- Davey, and the
referee for valuable comments and suggestions that improved this paper.
This work was supported by Program 973 grant 2006CB806303, NSFC grants
40636031 and 10873030, and CAS grant KJCX2- YW-T04. J. L.' s work at CfA
was supported by NASA grant NNX07AL72G, when he visited CfA.
NR 71
TC 60
Z9 66
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1716
EP 1731
DI 10.1088/0004-637X/700/2/1716
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100066
ER
PT J
AU Haiman, Z
Kocsis, B
Menou, K
AF Haiman, Zoltan
Kocsis, Bence
Menou, Kristen
TI THE POPULATION OF VISCOSITY- AND GRAVITATIONAL WAVE-DRIVEN SUPERMASSIVE
BLACK HOLE BINARIES AMONG LUMINOUS ACTIVE GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE black hole physics; galaxies: nuclei; gravitational waves
ID X-RAY VARIABILITY; HISTORICAL LIGHT-CURVE; STELLAR OBJECT DISCS; NEWTON
DEEP SURVEY; FIELD-NORTH SURVEY; OPTICAL VARIABILITY; RADIO GALAXIES;
SDSS J092712.65+294344.0; OBSERVATIONAL EVIDENCE; ELLIPTIC GALAXIES
AB Supermassive black hole binaries (SMBHBs) in galactic nuclei are thought to be a common by-product of major galaxy mergers. We use simple disk models for the circumbinary gas and for the binary-disk interaction to follow the orbital decay of SMBHBs with a range of total masses (M) and mass ratios (q), through physically distinct regions of the disk, until gravitational waves (GWs) take over their evolution. Prior to the GW-driven phase, the viscous decay is generically in the stalled "secondary-dominated" regime. SMBHBs spend a non-negligible fraction of a fiducial time of 10(7) yr at orbital periods between days less than or similar to t(orb) less than or similar to yr, and we argue that they may be sufficiently common to be detectable, provided they are luminous during these stages. A dedicated optical or X-ray survey could identify coalescing SMBHBs statistically, as a population of periodically variable quasars, whose abundance obeys the scaling N-var proportional to t(var)(alpha) within a range of periods around t(var) similar to tens of weeks. SMBHBs with M less than or similar to 10(7) M-circle dot, with 0.5 less than or similar to alpha less than or similar to 1.5, would probe the physics of viscous orbital decay, whereas the detection of a population of higher-mass binaries, with alpha = 8/3, would confirm that their decay is driven by GWs. The lowest-mass SMBHBs (M less than or similar to 10(5-6) M-circle dot) enter the GW-driven regime at short orbital periods, when they are already in the frequency band of the Laser Interferometric Space Antenna (LISA). While viscous processes are negligible in the last few years of coalescence, they could reduce the amplitude of any unresolved background due to near-stationary LISA sources. We discuss modest constraints on the SMBHB population already available from existing data, and the sensitivity and sky coverage requirements for a detection in future surveys. SMBHBs may also be identified from velocity shifts in their spectra; we discuss the expected abundance of SMBHBs as a function of their orbital velocity.
C1 [Haiman, Zoltan; Menou, Kristen] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Kocsis, Bence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kocsis, Bence] Inst Adv Study, Princeton, NJ 08540 USA.
[Kocsis, Bence] Eotvos Lorand Univ, Inst Phys, H-1117 Budapest, Hungary.
RP Haiman, Z (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA.
RI Kocsis, Bence/C-3061-2013
OI Kocsis, Bence/0000-0002-4865-7517
FU Polanyi Program of the Hungarian National Office for Research and
Technology (NKTH); NASA ATFP [NNX08AH35G]; OTKA [68228]
FX Z. H. thanks George Djorgovski and Tuck Stebbins for stimulating
discussions, and Mamoru Doi and Tomoki Morokuma for sharing their Subaru
variability search results prior to publication, which originally
inspired this paper. We also thank Zsolt Frei and David Hogg for useful
comments, Chris Stubbs, Michael Strauss, and Richard Mushotzky for
advice on variability surveys, and the anonymous referee for comments
that significantly improved this paper. K. M. thanks the Aspen Center
for Physics, where a part of the work reported here was performed, for
their hospitality. This work was supported by the Polanyi Program of the
Hungarian National Office for Research and Technology (NKTH) and by NASA
ATFP grant NNX08AH35G. B. K. acknowledges support from OTKA grant 68228.
NR 107
TC 75
Z9 75
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 AUG 1
PY 2009
VL 700
IS 2
BP 1952
EP 1969
DI 10.1088/0004-637X/700/2/1952
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100081
ER
PT J
AU Di Francesco, J
Andre, P
Myers, PC
AF Di Francesco, James
Andre, Philippe
Myers, Philip C.
TI QUIESCENT DENSE GAS IN PROTOSTELLAR CLUSTERS: THE OPHIUCHUS A CORE (vol
617, pg 425, 2004)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID N2H+
C1 [Di Francesco, James] Herzberg Inst Astrophys, Natl Res Council Canada, Victoria, BC V9E 2E7, Canada.
[Andre, Philippe] CEA, CE Saclay, Serv Astrophys, DSM,DAPNIA, F-91191 Gif Sur Yvette, France.
[Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Di Francesco, J (reprint author), Herzberg Inst Astrophys, Natl Res Council Canada, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada.
NR 5
TC 2
Z9 2
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2009
VL 700
IS 2
BP 1994
EP 1994
DI 10.1088/0004-637X/700/2/1994
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 471ZU
UT WOS:000268098100085
ER
PT J
AU Agueros, MA
Heinke, C
Camilo, F
Kilic, M
Anderson, SF
Freire, P
Kleinman, SJ
Liebert, JW
Silvestri, NM
AF Agueeros, Marcel A.
Heinke, Craig
Camilo, Fernando
Kilic, Mukremin
Anderson, Scott F.
Freire, Paulo
Kleinman, Scot J.
Liebert, James W.
Silvestri, Nicole M.
TI NO NEUTRON STAR COMPANION TO THE LOWEST MASS SDSS WHITE DWARF
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: general; stars: individual (SDSS J091709.55+463821.8); white
dwarfs
ID PHOTON IMAGING CAMERA; DIGITAL SKY SURVEY; XMM-NEWTON; BINARIES;
CATALOG; EVOLUTION; PULSARS; HELIUM; SEARCH
AB SDSS J091709.55+463821.8 (hereafter J0917+4638) is the lowest surface gravity white dwarf (WD) currently known, with log g = 5.55 +/- 0.05 (M approximate to 0.17 M(circle dot)). Such low-mass white dwarfs (LMWDs) are believed to originate in binaries that evolve into WD/WD or WD/neutron star (NS) systems. An optical search for J0917+4638's companion showed that it must be a compact object with a mass >= 0.28 M(circle dot). Here we report on Green Bank Telescope 820 MHz and XMM-Newton X-ray observations of J0917+4638 intended to uncover a potential NS companion to the LMWD. No convincing pulsar signal is detected in our radio data. Our X-ray observation also failed to detect X-ray emission from J0917+4638's companion, while we would have detected any of the millisecond radio pulsars in 47 Tuc. We conclude that the companion is almost certainly another WD.
C1 [Agueeros, Marcel A.; Camilo, Fernando] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Heinke, Craig] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Kilic, Mukremin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Anderson, Scott F.; Silvestri, Nicole M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Freire, Paulo] Arecibo Observ, Arecibo, PR 00612 USA.
[Kleinman, Scot J.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
[Liebert, James W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Agueros, MA (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM marcel@astro.columbia.edu
RI Agueros, Marcel/K-7998-2014;
OI Agueros, Marcel/0000-0001-7077-3664; Heinke, Craig/0000-0003-3944-6109
FU NSF [AST-0602099]; NSERC; Spitzer Space Telescope Fellowship Program;
JPL/Caltech under a contract with NASA; ESA Member States; NASA
FX M. A. A. is supported by an NSF Astronomy and Astrophysics Postdoctoral
Fellowship under award AST-0602099. C. H. is supported by NSERC. Further
support was provided to M. K. through the Spitzer Space Telescope
Fellowship Program, through a contract issued by the JPL/Caltech under a
contract with NASA.; The Robert C. Byrd Green Bank Telescope is operated
by the National Radio Astronomy Observatory, which is a facility of the
US National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. XMM-Newton is an ESA science mission with
instruments and contributions directly funded by ESA Member States and
NASA.
NR 35
TC 10
Z9 10
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2009
VL 700
IS 2
BP L123
EP L126
DI 10.1088/0004-637X/700/2/L123
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 472UJ
UT WOS:000268157500015
ER
PT J
AU Sakamoto, K
Aalto, S
Wilner, DJ
Black, JH
Conway, JE
Costagliola, F
Peck, AB
Spaans, M
Wang, JZ
Wiedner, MC
AF Sakamoto, Kazushi
Aalto, Susanne
Wilner, David J.
Black, John H.
Conway, John E.
Costagliola, Francesco
Peck, Alison B.
Spaans, Marco
Wang, Junzhi
Wiedner, Martina C.
TI P CYGNI PROFILES OF MOLECULAR LINES TOWARD ARP 220 NUCLEI
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: individual (Arp 220)
ID SUBMILLIMETER ARRAY; INFRARED GALAXIES; ARP-220; EMISSION; DIAGNOSTICS;
STARBURSTS; LUMINOSITY; SUPERNOVAE; CONTINUUM; OUTFLOWS
AB We report similar to 100 pc (0 ''.3) resolution observations of (sub) millimeter HCO(+) and CO lines in the ultraluminous infrared galaxy Arp 220. The lines peak at two merger nuclei, with HCO(+) being more spatially concentrated than CO. Asymmetric line profiles with blueshifted absorption and redshifted emission are discovered in HCO(+)(3-2) and (4-3) toward the two nuclei and in CO(3-2) toward one nucleus. We suggest that these P Cygni profiles are due to similar to 100 km s(-1) outward motion of molecular gas from the nuclei. This gas is most likely outflowing from the inner regions of the two nuclear disks rotating around individual nuclei, clearing the shroud around the luminosity sources there.
C1 [Sakamoto, Kazushi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Aalto, Susanne; Black, John H.; Conway, John E.; Costagliola, Francesco] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, SE-43992 Onsala, Sweden.
[Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Peck, Alison B.] Joint ALMA Observ, Santiago 7550108, Chile.
[Spaans, Marco] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Wang, Junzhi] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Wiedner, Martina C.] Observ Paris, F-75014 Paris, France.
RP Sakamoto, K (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM ksakamoto@asiaa.sinica.edu.tw
FU Smithsonian Institution; Academia Sinica
FX The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics, and is funded by the Smithsonian Institution and the
Academia Sinica.
NR 28
TC 46
Z9 46
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2009
VL 700
IS 2
BP L104
EP L108
DI 10.1088/0004-637X/700/2/L104
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 472UJ
UT WOS:000268157500011
ER
PT J
AU Schmit, DJ
Gibson, SE
Tomczyk, S
Reeves, KK
Sterling, AC
Brooks, DH
Williams, DR
Tripathi, D
AF Schmit, D. J.
Gibson, S. E.
Tomczyk, S.
Reeves, K. K.
Sterling, Alphonse C.
Brooks, D. H.
Williams, D. R.
Tripathi, D.
TI LARGE-SCALE FLOWS IN PROMINENCE CAVITIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: atmospheric motions; Sun: corona; Sun: prominences; Sun: UV
radiation
ID QUIESCENT PROMINENCE; FILAMENT; TEMPERATURES; CONDENSATION; DENSITIES;
DYNAMICS; HINODE; FIELDS; CORONA
AB Regions of rarefied density often form cavities above quiescent prominences. We observed two different cavities with the Coronal Multichannel Polarimeter on 2005 April 21 and with Hinode/EIS on 2008 November 8. Inside both of these cavities, we find coherent velocity structures based on spectral Doppler shifts. These flows have speeds of 5-10 km s(-1), occur over length scales of tens of megameters, and persist for at least 1 hr. Flows in cavities are an example of the nonstatic nature of quiescent structures in the solar atmosphere.
C1 [Schmit, D. J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Schmit, D. J.; Gibson, S. E.; Tomczyk, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sterling, Alphonse C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35805 USA.
[Brooks, D. H.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Williams, D. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Tripathi, D.] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
RP Schmit, DJ (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
RI Gibson, Sarah/A-9189-2011; Williams, David/E-6676-2011; Tripathi,
Durgesh/D-9390-2012; Reeves, Katharine/P-9163-2014
OI Williams, David/0000-0001-9922-8117; Tripathi,
Durgesh/0000-0003-1689-6254;
FU NASA [NNM07AB07C]
FX This work benefited from discussions of the International Working Group
on coronal prominence cavities sponsored by the International Space
Science Institute (ISSI). SOHO is a project of international cooperation
between ESA and NASA. Hinode is a Japanesemission developed and launched
by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in cooperation
with ESA and NSC (Norway). K. K. R. is supported by NASA contract
NNM07AB07C to SAO.
NR 21
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2009
VL 700
IS 2
BP L96
EP L98
DI 10.1088/0004-637X/700/2/L96
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 472UJ
UT WOS:000268157500009
ER
PT J
AU Taylor, EN
Franx, M
van Dokkum, PG
Quadri, RF
Gawiser, E
Bell, EF
Barrientos, LF
Blanc, GA
Castander, FJ
Damen, M
Gonzalez-Perez, V
Hall, PB
Herrera, D
Hildebrandt, H
Kriek, M
Labbe, I
Lira, P
Maza, J
Rudnick, G
Treister, E
Urry, CM
Willis, JP
Wuyts, S
AF Taylor, Edward N.
Franx, Marijn
van Dokkum, Pieter G.
Quadri, Ryan F.
Gawiser, Eric
Bell, Eric F.
Barrientos, L. Felipe
Blanc, Guillermo A.
Castander, Francisco J.
Damen, Maaike
Gonzalez-Perez, Violeta
Hall, Patrick B.
Herrera, David
Hildebrandt, Hendrik
Kriek, Mariska
Labbe, Ivo
Lira, Paulina
Maza, Jose
Rudnick, Gregory
Treister, Ezequiel
Urry, C. Megan
Willis, Jon P.
Wuyts, Stijn
TI A PUBLIC, K-SELECTED, OPTICAL-TO-NEAR-INFRARED CATALOG OF THE EXTENDED
CHANDRA DEEP FIELD SOUTH (ECDFS) FROM THE MULTIWAVELENGTH SURVEY BY
YALE-CHILE (MUSYC)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: distances and redshifts; galaxies: fundamental
parameters; galaxies: high-redshift; galaxies: photometry; surveys
ID EARLY-TYPE GALAXIES; ESO IMAGING SURVEY; HIGH-REDSHIFT GALAXIES;
STAR-FORMING GALAXIES; PHOTOMETRIC REDSHIFTS; MULTICOLOR CATALOG; RED
GALAXIES; DATA RELEASE; K20 SURVEY; SPECTROSCOPY
AB We present a new, K-selected, optical-to-near infrared photometric catalog of the Extended Chandra Deep Field South (ECDFS), making it publicly available to the astronomical community.(22) The data set is founded on publicly available imaging, supplemented by original z' JK imaging data collected as part of the MUltiwavelength Survey by Yale-Chile (MUSYC). The final photometric catalog consists of photometry derived from U U (38) BVRIz' JK imaging covering the full 1/2 x 1/2 square degrees. of the ECDFS, plus H-band photometry for approximately 80% of the field. The 5 sigma flux limit for point sources is K(tot)((AB)) = 22.0. This is also the nominal completeness and reliability limit of the catalog: the empirical completeness for 21.75 < K < 22.00 is greater than or similar to 85%. We have verified the quality of the catalog through both internal consistency checks, and comparisons to other existing and publicly available catalogs. As well as the photometric catalog, we also present catalogs of photometric redshifts and rest-frame photometry derived from the 10-band photometry. We have collected robust spectroscopic redshift determinations from published sources for 1966 galaxies in the catalog. Based on these sources, we have achieved a (1 sigma) photometric redshift accuracy of Delta z/(1 + z) = 0.036, with an outlier fraction of 7.8%. Most of these outliers are X-ray sources. Finally, we describe and release a utility for interpolating rest-frame photometry from observed spectral energy distributions, dubbed InterRest.(23)
C1 [Taylor, Edward N.; Franx, Marijn; Quadri, Ryan F.; Damen, Maaike; Hildebrandt, Hendrik] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[van Dokkum, Pieter G.; Herrera, David; Urry, C. Megan] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA.
[Bell, Eric F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Barrientos, L. Felipe] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile.
[Blanc, Guillermo A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Castander, Francisco J.; Gonzalez-Perez, Violeta] CSIC, Inst Ciencies Espai, IEEC, Fac Ciencies, Barcelona 08193, Spain.
[Hall, Patrick B.] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada.
[Kriek, Mariska] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Labbe, Ivo] Carnegie Observ, Pasadena, CA 91101 USA.
[Lira, Paulina; Maza, Jose] Univ Chile, Dept Astron, Santiago, Chile.
[Rudnick, Gregory] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Treister, Ezequiel] European So Observ, Santiago 19, Chile.
[Treister, Ezequiel] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Willis, Jon P.] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada.
[Wuyts, Stijn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Taylor, EN (reprint author), Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
EM ent@strw.leidenuniv.nl
RI Urry, Claudia/G-7381-2011; Taylor, Edward/C-6458-2015; Lira,
Paulina/G-8536-2016; Maza, Jose/I-5722-2016; Blanc,
Guillermo/I-5260-2016;
OI Urry, Claudia/0000-0002-0745-9792; Taylor, Edward/0000-0002-3958-0343;
Maza, Jose/0000-0003-2068-1328; Bell, Eric/0000-0002-5564-9873
NR 77
TC 100
Z9 101
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2009
VL 183
IS 2
BP 295
EP 319
DI 10.1088/0067-0049/183/2/295
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 479NH
UT WOS:000268665900009
ER
PT J
AU Valencia, D
O'Connell, RJ
Sasselov, DD
AF Valencia, Diana
O'Connell, Richard J.
Sasselov, Dimitar D.
TI The role of high-pressure experiments on determining super-Earth
properties
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article; Proceedings Paper
CT 7th International Conference on High Energy Density Laboratory
Astrophysics
CY APR 11-15, 2008
CL St Louis, MO
SP HEDLA, Amer Phys Soc
DE Equation of state; Super-Earths; Internal structure; Exoplanets
ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; NEPTUNE-MASS PLANETS; HARPS SEARCH;
SOLID EXOPLANETS; RADIUS; SYSTEM; EQUATION; MODELS
AB Super-Earths are the newest class of extra-solar planets with a mass range between about 1-10M (aS center dot) . With their large masses, they experience very large internal pressures. The central pressure scales proportionately with mass, reaching values that require us to extend our understanding of rock and H(2)O behavior to such extreme conditions. Pressure also constrains the power law relationship between mass and radius of solid planets R similar to M (beta) . The value for the exponent is 0.262a parts per thousand currency sign beta a parts per thousand currency sign0.274 as constrained by the different internal structure models for super-Earths, while it is 0.3 for planets between 5-50% the mass of Earth. Despite uncertainties in planetary composition, temperature structure and equation of state, the mass-radius relationship is robust, and thus, useful for inferring the expected signal in transit searches.
In the next few years many super-Earths will be discovered and their masses and radii will be known with some uncertainty. Even without errors in both the data and structure models, a large number of compositions can fit the same average density. However, the follow-up observations with space telescopes will yield very precise radius measurements and even probe the atmospheres of super-Earths. This radius uncertainty will then be comparable to the current error derived from the equation of state used by the structure models. Thus, there is a need for accurate equations of state of solid planetary materials. Furthermore, information on the structure, such as the size and state of the core, crucially depends on the exact behavior of super-Earth materials (i.e. silicates, iron, iron alloy and ices) at high pressures and temperatures. In addition, information about the atmospheric composition of these planets may prove useful in constraining their interiors. Ultimately any inference on the structure of super-Earths, including information from atmospheres, depends on the precision of interior models, which in turn require accurate equations of state.
C1 [Valencia, Diana; O'Connell, Richard J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Valencia, D (reprint author), Observ Cote Azur, BP 4229, F-06304 Nice, France.
EM valencia@eps.harvard.edu
NR 26
TC 12
Z9 12
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD AUG
PY 2009
VL 322
IS 1-4
BP 135
EP 139
DI 10.1007/s10509-009-0034-6
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 461TA
UT WOS:000267293200023
ER
PT J
AU Oprea, M
Mendes, P
Vieira, TB
Ditchfield, AD
AF Oprea, Monik
Mendes, Poliana
Vieira, Thiago B.
Ditchfield, Albert D.
TI Do wooded streets provide connectivity for bats in an urban landscape?
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE Chiroptera; Corridors; Habitat fragmentation; Habitat use; Urbanization;
Urban planning
ID FRUIT-EATING BAT; SPECIES ENDANGERMENT; ARTIBEUS-LITURATUS;
INSECTIVOROUS BATS; UNITED-STATES; HABITAT USE; CONSERVATION;
BIODIVERSITY; COMMUNITIES; FOREST
AB The effects of urbanization on bats are poorly understood, but published data suggests it might be detrimental to them. Even though urban parks provide refuge to native biota, the nature of the urban landscape exacerbates the insularization process. In order to evaluate if wooded streets in an urban landscape provide connectivity for bats, we compared bat community structure in three different types of habitats: urban parks, wooded streets and non-wooded streets. Sampling occurred monthly from August 2006 to July 2007 in the city of Vitria, southeastern Brazil. Richness, relative abundance and diversity were higher in urban parks and lower in non-wooded streets. Jaccard's similarity index showed that the wooded streets are more similar to non-wooded streets than to urban parks. Urbanization may benefit generalist species by providing new resources, but for specialist species critical resources may be lost and persistence endangered. There is evidence that wooded streets may provide some degree of connectivity for birds in urban landscapes, but our results suggest that this is not the case, with wooded streets being used by few individuals of a few species. Vegetation cover is important to maintain bat diversity in urban centers. Activities like landscape planning and gardening should include biodiversity data in their outputs in order to better design a landscape that improves the likelihood of persistence of bats.
C1 [Oprea, Monik] Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20013 USA.
[Oprea, Monik; Mendes, Poliana; Vieira, Thiago B.; Ditchfield, Albert D.] Univ Fed Espirito Santo, Dept Biol, Lab Chiroptera Studies, BR-29040090 Vitoria, Espirito Santo, Brazil.
RP Oprea, M (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, MRC 108, Washington, DC 20013 USA.
EM monik.bats@gmail.com; polimendes@gmail.com; thiagobernardi007@gmail.com;
trachops@gmail.com
RI Oprea, Monik/E-6204-2010; Vieira, Thiago/P-5233-2015
OI Vieira, Thiago/0000-0003-1762-8294
FU Bat Conservation International
FX We would like to thank our collegues Vinicius Pimenta, Marcio Almeida,
Silvia Ramira, Ricardo M. Fonseca, Rafael Z. Coutinho, and Geovana
Mendes for all the help on the fieldwork. Daniel Brito for reviewing
this manuscript prior to submission. Pedro L. Peloso for helping with
the map. We also thank Prefeitura Municipal de Vitoria and park managers
for fieldwork permission. Instituto Brasileiro do Meio Ambiente e dos
Recursos Naturais Renovaveis for the research authorization. M. Oprea
recieved a scholarship from Bat Conservation International through the
Student Research Scholarship.
NR 61
TC 15
Z9 23
U1 5
U2 68
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3115
EI 1572-9710
J9 BIODIVERS CONSERV
JI Biodivers. Conserv.
PD AUG
PY 2009
VL 18
IS 9
BP 2361
EP 2371
DI 10.1007/s10531-009-9593-7
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 473FB
UT WOS:000268190300007
ER
PT J
AU Muratori, FB
Gagne, RJ
Messing, RH
AF Muratori, Frederic B.
Gagne, Raymond J.
Messing, Russell H.
TI Ecological traits of a new aphid parasitoid, Endaphis fugitiva (Diptera:
Cecidomyiidae), and its potential for biological control of the banana
aphid, Pentalonia nigronervosa (Hemiptera: Aphididae)
SO BIOLOGICAL CONTROL
LA English
DT Article
DE Aphid; Parasitoid; Endaphis fugitiva; Cecidomyiidae; Diptera; Banana
aphid; Pentalonia nigronervosa; Biological control; Behavioral ecology
ID GALL-MIDGE; INSECT PARASITOIDS; SOIL TYPE; OVIPOSITION; PARAMETERS;
COLEMANI; SURVIVAL; MOISTURE; IMPACT; DEPTH
AB Most parasitoids of aphids are small wasps belonging to the families Braconidae or Aphelinidae. However, some dipteran parasitoids are also known to use aphids as hosts. We describe and give life-history information on a new species of aphid parasitoid, Endaphis fugitiva Gagne and Muratori, found to parasitize the banana aphid, Pentalonia nigronervosa Coquerel, the vector of banana bunchy top virus. Field and laboratory observations show that fly eggs are laid on the leaves near an aphid colony, the newly hatched fly larvae search for hosts while crawling on the leaf, and then penetrate the aphid between the legs and thorax. They develop as koinobiont endoparasitoids, and eventually emerge from the aphid anus and fall to the ground to pupate in the soil. We provide data relevant to parasitoid rearing on patterns of emergence, adult longevity, and effects of pupation substrate on adult emergence rate, and we discuss the potential of this new species to contribute to the biocontrol of banana aphid in Hawaii. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Muratori, Frederic B.] Univ Catholique Louvain, Biodivers Res Ctr, B-1348 Louvain, Belgium.
[Muratori, Frederic B.; Messing, Russell H.] Univ Hawaii Manoa, Kauai Agr Res Ctr, Kapaa, HI 96746 USA.
[Gagne, Raymond J.] Agr Res Serv, Systemat Entomol Lab, USDA, Smithsonian Inst MRC 168, Washington, DC 20013 USA.
RP Muratori, FB (reprint author), Univ Catholique Louvain, Biodivers Res Ctr, 4 Croix Sud, B-1348 Louvain, Belgium.
EM frederic.muratori@uclouvain.be
FU USDA-CSREES-TSTAR (Tropical and Subtropical Agricultural Research); FNRS
(Fonds de la Recherche Scientifique, Belgium)
FX RJ.G. thanks P. Malikul for making slide preparations, Diana Marques for
electronically setting up the drawings and photographs of Figs. I and 2,
and Scott D. Whittaker, SEM Laboratory manager, Smithsonian Institution,
for his assistance with the scanning electron microscope. F.B.M. is
deeply indebted to Sophie Borlee for her help in the field collection
and laboratory work, David Damiens, Guy Boivin and Thierry Hance for
stimulating discussions, and Catherine Tauber for Hemerobiidae
identification. This research was supported by a grant from the
USDA-CSREES-TSTAR (Tropical and Subtropical Agricultural Research)
program to R.H.M. F.B.M. thanks the F.R.S-FNRS (Fonds de la Recherche
Scientifique, Belgium) for financial support.
NR 48
TC 6
Z9 6
U1 2
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1049-9644
J9 BIOL CONTROL
JI Biol. Control
PD AUG
PY 2009
VL 50
IS 2
BP 185
EP 193
DI 10.1016/j.biocontrol.2009.04.007
PG 9
WC Biotechnology & Applied Microbiology; Entomology
SC Biotechnology & Applied Microbiology; Entomology
GA 454NK
UT WOS:000266689000015
ER
PT J
AU Paar, WH
Cooper, MA
Hawthorne, FC
Moffatt, E
Gunter, ME
Roberts, AC
Dunn, PJ
AF Paar, Werner H.
Cooper, Mark A.
Hawthorne, Frank C.
Moffatt, Elizabeth
Gunter, Mickey E.
Roberts, Andrew C.
Dunn, Pete J.
TI BRAITHWAITEITE, NaCu5(TiSb)O-2(AsO4)(4)[AsO3(OH)](2)(H2O)(8), A NEW
MINERAL SPECIES FROM LAURANI, BOLIVIA
SO CANADIAN MINERALOGIST
LA English
DT Article
DE braithwaiteite; new mineral species; epithermal (vein-type) deposit;
optical data; electron-microprobe analysis; IR spectroscopy; X-ray data;
Laurani; Sica Sica; Bolivia
ID CRYSTAL-STRUCTURE
AB Braithwaiteite, NaCu5(Ti4+Sb5+)O-2(As5+O4)(4)[As5+O3(OH)](2)(H2O)(8), is a new and very rare secondary mineral of copper, discovered in the supergene zone of an epithermal Cu-Au-Ag deposit at Laurani, near Sica Sica, Bolivia. This deposit is the type locality for lammerite, described as a new species in 1981. Braithwaiteite is closely associated with lammerite, lavendulan-lemanskiite and quartz. It formed by oxidation of Sb-bearing enargite in an arid environment. Traces of pyrite, covellite, anatase, albite-oligoclase, kaolinite and a mineral of the chlorite group are present as well. Electron-microprobe analysis gives Na2O 1.7, CuO 25.8, FeO 0.2, TiO2 4.5, Sb2O5 11.7, As2O5 42.3, H2O (calc.) 10.17, for a total of 96.37 wt.%. The empirical formula based on the results of crystal-structure solution and refinement [34 anions and 2(OH) + 8H(2)O] is Na0.87Cu5.172+(Ti0.904+Sb1.155+)(Sigma 2.05)O-2 (As0.985+O4)(4)[As0.985+O3(OH)](2)(H2O)(8). The simplified formula is NaCu5(TiSb)O-2(AsO4)(4)[AsO3(OH)](2)(H2O)(8), which requires Na2O 2.04, CuO 26.13, TiO2 5.25, Sb2O5 10.63, As2O5 45.30, H2O 10.65, total 100.00 wt.%. Infrared spectroscopy indicates the presence of H2O and OH, and As-O and As-OH stretching vibrations. Single-crystal X-ray studies show braithwaiteite to be triclinic, space group P (1) over bar, a 7.0308(4), b 9.8823(5), c 10.6754(6) angstrom, alpha 106.973(1), beta 104.274(1), gamma 93.839(1)degrees, V 679.76(11) angstrom(3), Z = 1, and a:b:c = 0.7115:1:1.0803. The strongest seven X-ray powder-diffraction lines [d in angstrom(I)(hkl)] are: 9.825(100)(001), 5.887(50)(011), 4.635(30)((1) over bar 02), 3.354(30)(1 (2) over bar2), 3.232(30)((21) over bar1), 2.947(60)(022), 2.736(30)((22) over bar2). Two crystals of braithwaiteite were found, one on matrix and the other loose, each of them less than 1 mm in size, plus a few very minute fragments. The forms that could be determined with certainty include the following pinacoids: {001} dominant, {010} less prominent, {100}, {103} and {203}, all subordinate. The crystals are transparent and have a sky-blue color, a vitreous luster and a very pale blue streak. Braithwaiteite is brittle and has a perfect cleavage parallel to {001}. Optically, braithwaiteite is biaxial negative, 2V(meas) 59(2), 2V(calc) 65 degrees. Indices of refraction are alpha 1.698(2), beta 1.757(5), gamma 1.783(5) at 589.3 nm. The mineral is weakly pleochroic with pale blue to greenish blue hues. The hardness (Mohs) is similar to 2. Using the empirical formula and the unit-cell parameters derived from the single-crystal study, the calculated density is 3.753 g cm(-3). Braithwaiteite is named after Dr. Richard S. W. Braithwaite (born 1930), prominent chemist and mineralogist at the University of Manchester, U. K. The mineral and mineral name have been approved by the Commission on New Minerals, Nomenclature and Classification, IMA (2006-050).
C1 [Paar, Werner H.] Salzburg Univ, Dept Mat Engn & Phys Mineral, A-5020 Salzburg, Austria.
[Cooper, Mark A.; Hawthorne, Frank C.] Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada.
[Moffatt, Elizabeth] Canadian Conservat Inst, Ottawa, ON K1A 0M5, Canada.
[Gunter, Mickey E.] Univ Idaho, Dept Geol Sci, Moscow, ID 83844 USA.
[Roberts, Andrew C.] Geol Survey Canada, Ottawa, ON K1A 0E8, Canada.
[Dunn, Pete J.] Smithsonian Inst, Washington, DC 20560 USA.
RP Paar, WH (reprint author), Salzburg Univ, Dept Mat Engn & Phys Mineral, Hellbrunnerstr 34, A-5020 Salzburg, Austria.
EM frank_hawthorne@umanitoba.ca
RI Hawthorne, Frank/F-6864-2011
OI Hawthorne, Frank/0000-0001-6405-9931
NR 15
TC 2
Z9 2
U1 0
U2 2
PU MINERALOGICAL ASSOC CANADA
PI QUEBEC
PA 490, RUE DE LA COURONNE, QUEBEC, QC G1K 9A9, CANADA
SN 0008-4476
J9 CAN MINERAL
JI Can. Mineral.
PD AUG
PY 2009
VL 47
IS 4
BP 947
EP 952
DI 10.3749/canmin.47.4.947
PG 6
WC Mineralogy
SC Mineralogy
GA 493HD
UT WOS:000269726000016
ER
PT J
AU Moyle, RG
Chesser, RT
Brumfield, RT
Tello, JG
Marchese, DJ
Cracraft, J
AF Moyle, Robert G.
Chesser, R. Terry
Brumfield, Robb T.
Tello, Jose G.
Marchese, Daniel J.
Cracraft, Joel
TI Phylogeny and phylogenetic classification of the antbirds, ovenbirds,
woodcreepers, and allies (Aves: Passeriformes: infraorder Furnariides)
SO CLADISTICS
LA English
DT Review
ID LENGTH DIFFERENCE TEST; DNA SEQUENCE DATA; MOLECULAR SYSTEMATICS;
PASSERINE BIRDS; NUCLEAR-DNA; BIOGEOGRAPHIC IMPLICATIONS; NEST
ARCHITECTURE; BAYES FACTORS; AVIAN FAMILY; INCONGRUENCE
AB The infraorder Furnariides is a diverse group of suboscine passerine birds comprising a substantial component of the Neotropical avifauna. The included species encompass a broad array of morphologies and behaviours, making them appealing for evolutionary studies, but the size of the group (ca. 600 species) has limited well-sampled higher-level phylogenetic studies. Using DNA sequence data from the nuclear RAG-1 and RAG-2 exons, we undertook a phylogenetic analysis of the Furnariides sampling 124 (more than 88%) of the genera. Basal relationships among family-level taxa differed depending on phylogenetic method, but all topologies had little nodal support, mirroring the results from earlier studies in which discerning relationships at the base of the radiation was also difficult. In contrast, branch support for family-rank taxa and for many relationships within those clades was generally high. Our results support the Melanopareidae and Grallariidae as distinct from the Rhinocryptidae and Formicariidae, respectively. Within the Furnariides our data contradict some recent phylogenetic hypotheses and suggest that further study is needed to resolve these discrepancies. Of the few genera represented by multiple species, several were not monophyletic, indicating that additional systematic work remains within furnariine families and must include dense taxon sampling. We use this study as a basis for proposing a new phylogenetic classification for the group and in the process erect new family-group names for clades having high branch support across methods.
C1 [Moyle, Robert G.; Tello, Jose G.; Marchese, Daniel J.; Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA.
[Moyle, Robert G.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
[Moyle, Robert G.] Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66045 USA.
[Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA.
[Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Tello, Jose G.] Long Isl Univ, Dept Biol, Brooklyn, NY 11201 USA.
RP Moyle, RG (reprint author), Amer Museum Nat Hist, Dept Ornithol, Cent Pk W & 79th St, New York, NY 10024 USA.
EM moyle@ku.edu
OI Brumfield, Robb/0000-0003-2307-0688
FU National Science Foundation [EAR-0228693, NSF DEB-0543562]; L. J. and L.
C. Sanford Funds; Lewis B. and Dorothy Cullman Program for Molecular
Systematic Studies; New York Botanical Gardens and the American Museum
of Natural History; Sackler Institute of Comparative Genomics, AMNH
FX We thank the following institutions for generous tissue loans: Field
Museum of Natural History, US National Museum of Natural History, and
the Zoological Museum at the University of Copenhagen. We also thank all
of the field collectors whose efforts made this project possible.
Richard C. Banks (Smithsonian Institution) provided invaluable comments
and advice on nomenclatural issues for which we are deeply grateful.
This research was supported by grants from the National Science
Foundation ("Assembling the Tree of Life" EAR-0228693, and NSF
DEB-0543562). These studies were also supported by the L. J. and L. C.
Sanford Funds, and the Lewis B. and Dorothy Cullman Program for
Molecular Systematic Studies, a joint initiative of the New York
Botanical Gardens and the American Museum of Natural History, as well as
by the Sackler Institute of Comparative Genomics, AMNH.
NR 102
TC 38
Z9 40
U1 2
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0748-3007
EI 1096-0031
J9 CLADISTICS
JI Cladistics
PD AUG
PY 2009
VL 25
IS 4
BP 386
EP 405
DI 10.1111/j.1096-0031.2009.00259.x
PG 20
WC Evolutionary Biology
SC Evolutionary Biology
GA 471IY
UT WOS:000268051800003
ER
PT J
AU Lance, SL
Hagen, C
Glenn, TC
Brumfield, RT
Stryjewski, KF
Graves, GR
AF Lance, Stacey L.
Hagen, Cris
Glenn, Travis C.
Brumfield, Robb T.
Stryjewski, Katherine Faust
Graves, Gary R.
TI Fifteen polymorphic microsatellite loci from Jamaican streamertail
hummingbirds (Trochilus)
SO CONSERVATION GENETICS
LA English
DT Article
DE Black-billed streamertail; Hummingbird; Jamaica; Microsatellite; PCR
primers; SSR; STR; Red-billed streamertail; Trochilus polytmus;
Trochilus scitulus
AB We isolated and characterized 15 microsatellite loci from the endemic Jamaican streamertail hummingbird Trochilus polytmus. Loci were screened in 12 individuals of both T. polytmus and its sister species T. scitulus, also a Jamaican endemic. The number of alleles per locus ranged from 2 to 10, observed heterozygosity ranged from 0 to 1, and the probability of identity values ranged from 0.038 to 0.663. These new loci provide tools for characterizing the narrow hybrid zone between the two species.
C1 [Brumfield, Robb T.; Stryjewski, Katherine Faust] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Lance, Stacey L.; Glenn, Travis C.] Univ Georgia, Dept Environm Hlth Sci, Athens, GA 30602 USA.
[Lance, Stacey L.; Hagen, Cris] Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA.
[Brumfield, Robb T.; Stryjewski, Katherine Faust] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA.
RP Brumfield, RT (reprint author), Louisiana State Univ, Museum Nat Sci, 119 Foster Hall, Baton Rouge, LA 70803 USA.
EM brumfld@lsu.edu
RI Glenn, Travis/A-2390-2008; Lance, Stacey/K-9203-2013; Brumfield,
Robb/K-6108-2015
OI Lance, Stacey/0000-0003-2686-1733; Brumfield, Robb/0000-0003-2307-0688
NR 11
TC 6
Z9 6
U1 1
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1566-0621
J9 CONSERV GENET
JI Conserv. Genet.
PD AUG
PY 2009
VL 10
IS 4
BP 1195
EP 1198
DI 10.1007/s10592-008-9748-1
PG 4
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 459LN
UT WOS:000267104000068
ER
PT J
AU Santos-Granero, F
AF Santos-Granero, Fernando
TI Hybrid Bodyscapes A Visual History of Yanesha Patterns of Cultural
Change
SO CURRENT ANTHROPOLOGY
LA English
DT Review
ID POLITICS; PERSPECTIVISM; PEOPLE; WOMEN
AB This paper examines cultural change and hybridity through a visual history of the alterations in dress, ornamentation, and body treatment experienced by the Yanesha of Peruvian Amazonia in postcolonial times. Such transformations often appear to be fluctuations between tradition and modernity explained alternatively as instances of "acculturation" or as expressions of "invented traditions" and "postmodern identity politics." By focusing mainly on external factors, these theoretical approaches pay insufficient attention to the role of native perceptions and practices in promoting cultural change. Approaches that do take into consideration these perceptions, such as those centered on the notions of "passing" and "mimesis," do not apply to this particular case. Adopting a Yanesha perspective as a departure point, I argue that what appear to be expressions of acculturative processes are the result of a long-standing indigenous openness to the Other-particularly the white and mestizo Others-and the native conviction that the Self is possible only through the incorporation of the Other. Such incorporation always finds expression in bodily transformations, hybrid bodyscapes that change throughout time according to the shifting relationships between Self and Other.
C1 Smithsonian Trop Res Inst, Dpo, AA 34002 USA.
RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, Dpo, AA 34002 USA.
EM santosf@si.edu
NR 115
TC 16
Z9 19
U1 1
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0011-3204
J9 CURR ANTHROPOL
JI Curr. Anthropol.
PD AUG
PY 2009
VL 50
IS 4
BP 477
EP 512
DI 10.1086/604708
PG 36
WC Anthropology
SC Anthropology
GA 464IJ
UT WOS:000267498300003
ER
PT J
AU Murphy, PNC
Bell, A
Turner, BL
AF Murphy, P. N. C.
Bell, A.
Turner, B. L.
TI Phosphorus speciation in temperate basaltic grassland soils by solution
P-31 NMR spectroscopy
SO EUROPEAN JOURNAL OF SOIL SCIENCE
LA English
DT Article
ID NUCLEAR-MAGNETIC-RESONANCE; PLANT-AVAILABLE PHOSPHORUS; NAOH-EDTA
EXTRACTION; ORGANIC PHOSPHORUS; PASTURE SOILS; PHOSPHATASE-ACTIVITIES;
SEQUENTIAL EXTRACTION; CHEMICAL NATURE; MOUNTAIN SOILS; NEW-ZEALAND
AB P>Phosphorus (P) speciation in 21 basaltic and four non-basaltic Irish grassland soils was determined by NaOH-EDTA extraction and P-31 NMR spectroscopy. Organic P in basaltic soils ranged between 30 and 697 mg P kg(-1) and consisted of phosphate monoesters (84-100%), DNA (0-16%) and phosphonates (0-5%). Inorganic P was mainly phosphate (83-100%) with small concentrations of pyrophosphate (0-17%). Phosphate monoesters were more important as a proportion of extracted P in basaltic soils, probably because of their greater oxalate-extractable Fe and Al contents. Phosphate monoesters appeared to be strongly associated with non-crystalline Al and increased with total soil P concentration, indicating that they do accumulate in grassland soils. In non-basaltic soils myo-inositol hexakisphosphate constituted between 20 and 52% of organic P, while scyllo-inositol hexakisphosphate constituted between 12 and 17%. These compounds were not quantified separately in basaltic soils because of poor NMR resolution in the phosphate monoester region, but appeared to represent a considerable proportion of the organic P in most samples. DNA concentrations were greater in basaltic soils compared with non-basaltic soils and were associated with acidic pH and large total C contents. The inability of the Olsen P test to assess effectively the P status of basaltic soils may result from strong phosphate sorption to Fe and Al oxides, inducing plant utilization of soil organic P. Phosphorus nutrient management should account for this to avoid over-application of P and associated financial and environmental costs.
C1 [Murphy, P. N. C.] TEAGASC, Moorepk Res Ctr, Fermoy, Cork, Ireland.
[Bell, A.] Belfast Royal Acad, Belfast BT14 6JL, Antrim, North Ireland.
[Turner, B. L.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Murphy, PNC (reprint author), TEAGASC, Moorepk Res Ctr, Fermoy, Cork, Ireland.
EM paul.murphy@teagasc.ie
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
FU Thomas Henry Foundation; Agricultural Research Service of the United
States Department of Agriculture
FX We acknowledge the contribution of Dr R.J. Stevens and Dr J. Bailey, and
thank Alex Blumenfeld (University of Idaho) and the laboratory staff at
Queen's University Belfast for analytical support. This work was funded
by the Thomas Henry Foundation and the Agricultural Research Service of
the United States Department of Agriculture.
NR 77
TC 28
Z9 31
U1 1
U2 24
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1351-0754
J9 EUR J SOIL SCI
JI Eur. J. Soil Sci.
PD AUG
PY 2009
VL 60
IS 4
BP 638
EP 651
DI 10.1111/j.1365-2389.2009.01148.x
PG 14
WC Soil Science
SC Agriculture
GA 470CC
UT WOS:000267949500014
ER
PT J
AU DeVorkin, DH
AF DeVorkin, David H.
TI In the grip of the big telescope age
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
CT Conference on 400 Years of Astronomical Telescopes
CY SEP, 2008
CL Leiden, NETHERLANDS
SP Leiden Observ
DE Hale era; Telescope; Reflector; Refractor; Coude
ID OPTIMUM SIZE; ARCTURUS
AB George Ellery Hale was a man of many dreams. One of his most persistent was to find the means to collect as much light as possible, but there is another element in his designs for the modern astrophysical observatory that has even greater significance, as it defines and distinguishes the practice of astrophysics from that of classical astronomy. Here we examine factors that either impeded or drove the acceptance of reflectors over refractors around the turn of the twentieth century at the outset of what may best be called the "Hale era." This commenced in the late nineteenth century, when the first large multi-focus photographic reflectors emerged during the reign of the great refractors. It lasted through to the onset of World War II when astronomical practice was dominated by ten reflectors with mirrors between 60 and 100 in., and was about to add one more whose surface area would almost double that of all the rest combined. We will touch upon how design choice reflected both scientific priorities and technological limitations.
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP DeVorkin, DH (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
EM devorkind@si.edu
NR 61
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD AUG
PY 2009
VL 25
IS 1-3
BP 63
EP 77
DI 10.1007/s10686-009-9146-9
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 469KF
UT WOS:000267896100006
ER
PT J
AU Marra, PP
Dove, CJ
Dolbeer, R
Dahlan, NF
Heacker, M
Whatton, JF
Diggs, NE
France, C
Henkes, GA
AF Marra, Peter P.
Dove, Carla J.
Dolbeer, Richard
Dahlan, Nor Faridah
Heacker, Marcy
Whatton, James F.
Diggs, Nora E.
France, Christine
Henkes, Gregory A.
TI Migratory Canada geese cause crash of US Airways Flight 1549
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Article
ID BIRDS; HYDROGEN
AB In the United States alone, over 7400 bird-aircraft collisions (birdstrikes) were reported in 2007. Most of these strikes occurred during takeoff or landing of the flight, and it is during these flight phases that aircraft experience their highest risk of substantial damage after colliding with birds. Birdstrikes carry enormous potential costs in terms of lives and money. Using feather remains and other tissue samples collected from the engines of US Airways Flight 1549, which crash landed in the Hudson River in New York City on 15 January 2009 after a birdstrike, we apply molecular tools and stable hydrogen isotopes to demonstrate that migratory Canada geese were responsible for the crash. Determining whether the geese involved in this birdstrike event were resident or migratory is essential to the development of management techniques that could reduce the risk of future collisions. Currently, the US civil aviation industry is not required to report birdstrikes, yet information on frequency, timing, and species involved, as well as the geographic origin of the birds, is critical to reducing the number of birdstrikes. Integrating this information with bird migration patterns, bird-detecting radar, and bird dispersal programs at airports can minimize the risk of such collisions in the future.
C1 [Marra, Peter P.; Diggs, Nora E.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC USA.
[Dove, Carla J.; Dahlan, Nor Faridah; Heacker, Marcy; Whatton, James F.] Smithsonian Inst, Natl Museum Nat Hist, Feather Identificat Lab, Washington, DC 20560 USA.
[Dolbeer, Richard] Wildlife Serv, USDA, Sandusky, OH USA.
[France, Christine; Henkes, Gregory A.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD USA.
RP Marra, PP (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC USA.
EM marrap@si.edu
RI Henkes, Gregory/D-9751-2011
NR 26
TC 32
Z9 37
U1 2
U2 31
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1540-9295
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD AUG
PY 2009
VL 7
IS 6
BP 297
EP 301
DI 10.1890/090066
PG 5
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 480WF
UT WOS:000268767000017
ER
PT J
AU Angelier, F
Clement-Chastel, C
Welcker, J
Gabrielsen, GW
Chastel, O
AF Angelier, Frederic
Clement-Chastel, Celine
Welcker, Jorg
Gabrielsen, Geir Wing
Chastel, Olivier
TI How does corticosterone affect parental behaviour and reproductive
success? A study of prolactin in black-legged kittiwakes
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE corticosterone; kittiwake; parental care; prolactin; seabird; stress
ID VASOACTIVE-INTESTINAL-PEPTIDE; LONG-LIVED BIRD; TURKEY
MELEAGRIS-GALLOPAVO; BASE-LINE CORTICOSTERONE; BODY CONDITION;
INCUBATION BEHAVIOR; CLUTCH SIZE; ENVIRONMENTAL VARIABILITY;
SOMATERIA-MOLLISSIMA; PLASMA PROLACTIN
AB P>An emergency life-history stage is expressed in breeding vertebrates when the immediate survival is threatened by poor energetic conditions (i.e. allostatic overload). This emergency life-history stage shifts energy investment away from reproduction and redirects it toward immediate survival.
In birds, this emergency life-history stage is promoted by a release of the stress hormone corticosterone. However, how corticosterone reduces the expression of parental cares remains to be clarified. One hypothesis is that the release of corticosterone may also affect prolactin levels, a pituitary hormone widely involved in regulating parental behaviours.
We tested this hypothesis by experimentally increasing corticosterone levels of chick-rearing black-legged kittiwakes (Rissa tridactyla) over a 2-day period and by monitoring prolactin levels over an 8-day period. We also investigated whether this hormonal manipulation affected nest attendance, the motivation to come back to the nest after a short-term stress and breeding success.
Corticosterone treatment resulted in a significant increase in plasma corticosterone levels during the first 2 days, which returned to pre-treatment values at day 3. This short-term corticosterone increase was accompanied by a 30% decrease in prolactin levels. Prolactin levels were reduced in a progressive and persistent manner and did not return to their initial levels when corticosterone levels returned to pre-treatment levels. Moreover, although corticosterone levels had returned to pre-treatment values, low prolactin levels were associated with a reduced nest attendance and a greater latency to come back to the nest after a short-term stress. This hormonal treatment also significantly reduced breeding success.
This experimental treatment strongly supports the idea that the secretion of these two hormones might be mechanistically linked. Thus, we showed that even a relatively short-term increase in corticosterone levels can durably affect plasma prolactin levels. Therefore, the well-established suppressive action of corticosterone on parental behaviour is probably mediated and reinforced through an effect on prolactin levels. This study highlights the need to consider the potential synergistic effects of these two hormones when studying on the hormonal basis of parental decisions.
C1 [Angelier, Frederic; Clement-Chastel, Celine; Chastel, Olivier] CNRS, Ctr Etud Biol Chize, F-79360 Paris, France.
[Welcker, Jorg; Gabrielsen, Geir Wing] Norwegian Polar Res Inst, N-9296 Tromso, Norway.
RP Angelier, F (reprint author), Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM angelierf@si.edu
FU French Polar Institute (IPEV); CNRS/Region Poitou-Charentes
FX The present research project No 330 has been performed at the Ny
Alesund-Rabot Station and was supported by the French Polar Institute
(IPEV). F. Angelier was supported by a BDI grant from CNRS/Region
Poitou-Charentes. We are grateful to Dr. A.F. Parlow for kindly
providing us with a chicken kit for prolactin assay. We thank A.Z.
Lendvai and two anonymous referees for helpful comments on the
manuscript, S. Dano, A. Lacroix and C. Trouve for their technical
assistance in hormone assay and S.R. Sult for kindly improving the
English of the original version of the manuscript.
NR 74
TC 81
Z9 81
U1 5
U2 59
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0269-8463
J9 FUNCT ECOL
JI Funct. Ecol.
PD AUG
PY 2009
VL 23
IS 4
BP 784
EP 793
DI 10.1111/j.1365-2435.2009.01545.x
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 464WD
UT WOS:000267539000014
ER
PT J
AU Chen, HX
Sundberg, P
Norenburg, JL
Sun, SC
AF Chen, Hai-Xia
Sundberg, Per
Norenburg, Jon L.
Sun, Shi-Chun
TI The complete mitochondrial genome of Cephalothrix simula (Iwata)
(Nemertea: Palaeonemertea)
SO GENE
LA English
DT Article
DE mtDNA; Nemertean; Gene order; Phylogeny
ID RIBOSOMAL-RNA SEQUENCES; PHYLOGENETIC POSITION; LOPHOTROCHOZOAN
PHYLOGENY; MOLECULAR PHYLOGENY; CODON REASSIGNMENT; MAXIMUM-LIKELIHOOD;
GENE ARRANGEMENTS; ANIMAL PHYLOGENY; PHYLUM NEMERTEA; DNA-SEQUENCE
AB The first complete mitochondrial genome sequence for a nemertean, Cephalothrix simula, was determined by conventional and long PCR and sequencing with primer walking methods. This circular genome is 16,296 bp in size and encodes 37 genes (13 protein-coding genes, 2 ribosomal RNAs, and 22 transfer RNAs) typically found in metazoans. All genes are encoded on H-strand except two tRNAs (trnT and trnP). It differs from those reported for other metazoans. but some gene junctions are shared with those of other protostomes. Structure of the mitochondrial genome of C. simula is mostly concordant with the partial mitochondrial genome known for Cephalothrix rufifrons, but notable differences include three large indel events and transposition of 2 tRNAs. Nucleotide composition of the mitochondrial genome of C simula is highly A+T biased. The compositional skew is strongly reflected in the codon-usage patterns and the amino acid compositions of the mitochondrial proteins. An AT-rich noncoding region with potential to form stem-loop structures may be involved in the initiation of replication or transcription. Gene adjacencies and phylogenetic analysis based on the 12 concatenated amino acid sequences (except atp8) of mitochondrial protein-coding genes show that the nemertean is close to the coelomate lophotrochozoans, rather than the acoelomate platyhelminths. (C) 2009 Elsevier B.V. All rights reserved.
C1 [Chen, Hai-Xia; Sun, Shi-Chun] Ocean Univ China, Mariculture Res Lab, Qingdao 266003, Peoples R China.
[Sundberg, Per] Gothenburg Univ, Dept Zool, SE-40530 Gothenburg, Sweden.
[Norenburg, Jon L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Sun, SC (reprint author), Ocean Univ China, Mariculture Res Lab, 5 Yushan Rd, Qingdao 266003, Peoples R China.
EM sunsc@ouc.edu.cn
RI Norenburg, Jon/K-3481-2015
OI Norenburg, Jon/0000-0001-7776-1527
FU National Natural Science Foundation of China [30270235]; Swedish
Research Council
FX The study was supported by the National Natural Science Foundation of
China (30270235) and, the Swedish Research Council (travel grant to
HXC). We would like to thank Mr. Wei Shi and Xu-Zhen Wang for technical
assistance in analyzing the sequences.
NR 77
TC 16
Z9 18
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1119
J9 GENE
JI Gene
PD AUG 1
PY 2009
VL 442
IS 1-2
BP 8
EP 17
DI 10.1016/j.gene.2009.04.015
PG 10
WC Genetics & Heredity
SC Genetics & Heredity
GA 464BE
UT WOS:000267478600002
PM 19397957
ER
PT J
AU Angelier, F
Chastel, O
AF Angelier, Frederic
Chastel, Olivier
TI Stress, prolactin and parental investment in birds: A review
SO GENERAL AND COMPARATIVE ENDOCRINOLOGY
LA English
DT Article; Proceedings Paper
CT 9th International Symposium on Avian Endocrinology
CY JUL 11-15, 2008
CL Leuven, BELGIUM
DE Prolactin; Stress; Parental care; Parental effort; Birds
ID LONG-LIVED SEABIRD; VASOACTIVE-INTESTINAL-PEPTIDE; TURKEY
MELEAGRIS-GALLOPAVO; INCUBATION BEHAVIOR; CLUTCH SIZE; RING DOVES;
REPRODUCTIVE ENDOCRINOLOGY; SOMATERIA-MOLLISSIMA; LUTEINIZING-HORMONE;
BREEDING EXPERIENCE
AB In this paper, we review the relationships that link avian parental behavior, stress (acute or chronic) and energetic constraints to the secretion of prolactin, the 'parental hormone'. Prolactin secretion is stimulated by exposure of the parent to tactile and visual stimuli from the nest, the eggs or the chicks, while prolactin facilitates/stimulates the expression of parental behaviors, such as incubating, brooding or feeding. Because of this role of prolactin in the expression of parental behaviors, we suggest that absolute circulating prolactin levels may reflect to the extent to which individuals provide parental care (i.e., parental effort). Stressors and energetic constraints (acute or chronic) depress prolactin levels ('the prolactin stress response') and this may be adaptive because it may disrupt the current parental effort of an individual and promote its survival. Alternatively, an attenuation of the prolactin stress response can be considered as a hormonal tactic permitting the maintenance of parental care to the detriment of parental survival during stressful situations. Therefore, we suggest that the magnitude of the prolactin stress response may reflect parental investment. Finally, we detail the interaction that links corticosterone, prolactin and stress in bird parents. We suggest that corticosterone and prolactin may mediate different components of the stress response, and, therefore, we emphasize the importance of considering both hormones when investigating the hormonal basis of parental investment. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Angelier, Frederic; Chastel, Olivier] Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[Angelier, Frederic] CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, France.
RP Angelier, F (reprint author), Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
EM angelierf@si.edu
NR 68
TC 108
Z9 110
U1 8
U2 75
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0016-6480
J9 GEN COMP ENDOCR
JI Gen. Comp. Endocrinol.
PD AUG-SEP
PY 2009
VL 163
IS 1-2
BP 142
EP 148
DI 10.1016/j.ygcen.2009.03.028
PG 7
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 473NG
UT WOS:000268213200024
PM 19351537
ER
PT J
AU Stiling, P
Moon, D
Rossi, A
Hungate, BA
Drake, B
AF Stiling, Peter
Moon, Daniel
Rossi, Anthony
Hungate, Bruce A.
Drake, Bert
TI Seeing the forest for the trees: long-term exposure to elevated CO2
increases some herbivore densities
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE elevated CO2; insect densities; insect herbivory; Kennedy Space Center;
leaf production; long-term effects; oak trees; species-specific
responses
ID SCRUB-OAK ECOSYSTEM; ATMOSPHERIC CARBON-DIOXIDE; ABOVEGROUND BIOMASS;
INSECT HERBIVORY; FOLIAR QUALITY; PERFORMANCE; ENRICHMENT; RESPONSES;
PHOTOSYNTHESIS; CANOPY
AB The effects of elevated CO2 on plant growth and insect herbivory have been frequently investigated over the past 20 years. Most studies have shown an increase in plant growth, a decrease in plant nitrogen concentration, an increase in plant secondary metabolites and a decrease in herbivory. However, such studies have generally overlooked the fact that increases in plant production could cause increases of herbivores per unit area of habitat. Our study investigated leaf production, herbivory levels and herbivore abundance per unit area of leaf litter in a scrub-oak system at Kennedy Space Center, Florida, under conditions of ambient and elevated CO2, over an 11-year period, from 1996 to 2007. In every year, herbivory, that is leafminer and leaftier abundance per 200 leaves, was lower under elevated CO2 than ambient CO2 for each of three species of oaks, Quercus myrtifolia, Quercus chapmanii and Quercus geminata. However, leaf litter production per 0.1143 m(2) was greater under elevated CO2 than ambient CO2 for Q. myrtifolia and Q. chapmanii, and this difference increased over the 11 years of the study. Leaf production of Q. geminata under elevated CO2 did not increase. Leafminer densities per 0.1143 m(2) of litterfall for Q. myrtifolia and Q. chapmanii were initially lower under elevated CO2. However, shortly after canopy closure in 2001, leafminer densities per 0.1143 m(2) of litter fall became higher under elevated CO2 and remained higher for the remainder of the experiment. Leaftier densities per 0.1143 m(2) were also higher under elevated CO2 for Q. myrtifolia and Q. chapmanii over the last 6 years of the experiment. There were no differences in leafminer or leaftier densities per 0.1143 m(2) of litter for Q. geminata. These results show three phenomena. First, they show that elevated CO2 decreases herbivory on all oak species in the Florida scrub-oak system. Second, despite lower numbers of herbivores per 200 leaves in elevated CO2, increased leaf production resulted in higher herbivore densities per unit area of leaf litter for two oak species. Third, they corroborate other studies which suggest that the effects of elevated CO2 on herbivores are species specific, meaning they depend on the particular plant species involved. Two oak species showed increases in leaf production and herbivore densities per 0.1143 m(2) in elevated CO2 over time while another oak species did not. Our results point to a future world of elevated CO2 where, despite lower plant herbivory, some insect herbivores may become more common.
C1 [Stiling, Peter] Univ S Florida, Dept Biol, SCA 110, Tampa, FL 33620 USA.
[Moon, Daniel; Rossi, Anthony] Univ N Florida, Dept Biol, Jacksonville, FL 33224 USA.
[Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA.
[Drake, Bert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Stiling, P (reprint author), Univ S Florida, Dept Biol, SCA 110, 4202 E Fowler Ave, Tampa, FL 33620 USA.
EM pstiling@cas.usf.edu
RI Hungate, Bruce/F-8991-2011
OI Hungate, Bruce/0000-0002-7337-1887
FU Office of Science (BER), US Department of Energy, through the Southeast
Regional Center of the National Institute for Global Environmental
Change [DE-FGO2-95ER61993]; National Science Foundation [DEB 0445324]
FX This research was supported by the Office of Science (BER), US
Department of Energy, through the Southeast Regional Center of the
National Institute for Global Environmental Change grants to Peter
Stiling and by a National Science Foundation grant (DEB 0445324) to
Bruce Hungate and by Department of Energy grant (DE-FGO2-95ER61993) to
Bert Drake. Thanks to Sylvia Lukasiewicz, Terri Albarricin, Kerry Bohl
and Heather Jezorek for help in sorting leaf samples and to Ben Duval,
Paul Dijkstra, and Rick Doucett for help with the foliar nitrogen
analyses. We acknowledge the support and encouragement of NASA Kennedy
Space Center and Dynamac Corporation, especially Ross Hinkle. Comments
by an anonymous reviewer greatly improved the manuscript.
NR 41
TC 18
Z9 18
U1 1
U2 19
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD AUG
PY 2009
VL 15
IS 8
BP 1895
EP 1902
DI 10.1111/j.1365-2486.2009.01902.x
PG 8
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 466XL
UT WOS:000267698400004
ER
PT J
AU McKinley, DC
Romero, JC
Hungate, BA
Drake, BG
Megonigal, JP
AF McKinley, Duncan C.
Romero, Julio C.
Hungate, Bruce A.
Drake, Bert G.
Megonigal, James P.
TI Does deep soil N availability sustain long-term ecosystem responses to
elevated CO2?
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE deep soil nitrogen availability; elevated CO2; global change; gross N
mineralization; nitrogen cycling; progressive nitrogen limitation;
rising atmospheric CO2; water table
ID SCRUB-OAK ECOSYSTEM; PROGRESSIVE NITROGEN LIMITATION; ATMOSPHERIC
CARBON-DIOXIDE; FINE ROOTS; TERRESTRIAL ECOSYSTEMS; ABOVEGROUND BIOMASS;
TEMPERATE FOREST; DECIDUOUS FOREST; PINE FOREST; ENRICHMENT
AB A scrub-oak woodland has maintained higher aboveground biomass accumulation after 11 years of atmospheric CO2 enrichment (ambient 1350 mu mol CO2 mol(-1)), despite the expectation of strong nitrogen (N) limitation at the site. We hypothesized that changes in plant available N and exploitation of deep sources of inorganic N in soils have sustained greater growth at elevated CO2. We employed a suite of assays performed in the sixth and 11th year of a CO2 enrichment experiment designed to assess soil N dynamics and N availability in the entire soil profile. In the 11th year, we found no differences in gross N flux, but significantly greater microbial respiration (P <= 0.01) at elevated CO2. Elevated CO2 lowered extractable inorganic N concentrations (P=0.096) considering the whole soil profile (0-190 cm). Conversely, potential net N mineralization, although not significant in considering the entire profile (P=0.460), tended to be greater at elevated CO2. Ion-exchange resins placed in the soil profile for approximately 1 year revealed that potential N availability at the water table was almost 3 x greater than found elsewhere in the profile, and we found direct evidence using a 15 N tracer study that plants took up N from the water table. Increased microbial respiration and shorter mean residence times of inorganic N at shallower depths suggests that enhanced SOM decomposition may promote a sustained supply of inorganic N at elevated CO2. Deep soil N availability at the water table is considerable, and provides a readily available source of N for plant uptake. Increased plant growth at elevated CO2 in this ecosystem may be sustained through greater inorganic N supply from shallow soils and N uptake from deep soil.
C1 [McKinley, Duncan C.; Romero, Julio C.; Drake, Bert G.; Megonigal, James P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA.
RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM megonigalp@si.edu
RI Hungate, Bruce/F-8991-2011
OI Hungate, Bruce/0000-0002-7337-1887
FU National Science Foundation [DEB-0445324]
FX This work was supported by a grant from the National Science Foundation
(DEB-0445324). This project was accomplished with assistance and
tireless work from Nicolas Mudd, Todd Wojtowicz, James Brown, Joseph
Balnkinship, Ben Duval, and Jay Garland. We acknowledge the support of
NASA Kennedy Space Center, Dynamac 457 Corp., and US Fish and Wildlife
Service, Merritt Island National Wildlife Refuge.
NR 56
TC 23
Z9 26
U1 1
U2 39
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD AUG
PY 2009
VL 15
IS 8
BP 2035
EP 2048
DI 10.1111/j.1365-2486.2008.01836.x
PG 14
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 466XL
UT WOS:000267698400014
ER
PT J
AU Koehler, B
Corre, MD
Veldkamp, E
Wullaert, H
Wright, SJ
AF Koehler, Birgit
Corre, Marife D.
Veldkamp, Edzo
Wullaert, Hans
Wright, S. Joseph
TI Immediate and long-term nitrogen oxide emissions from tropical forest
soils exposed to elevated nitrogen input
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE climate change; deposition; fertilization; nitric oxide; nitrification;
nitrogen; nitrous oxide; organic layer; trace gases; tropical forest
ID MONTANE RAIN-FOREST; LOWLAND AMAZONIAN FOREST; NITRIC-OXIDE; NUTRIENT
LIMITATION; EASTERN AMAZONIA; CARBON-DIOXIDE; HUMID TROPICS; COSTA-RICA;
NO; ECOSYSTEM
AB Tropical nitrogen (N) deposition is projected to increase substantially within the coming decades. Increases in soil emissions of the climate-relevant trace gases NO and N2O are expected, but few studies address this possibility. We used N addition experiments to achieve N-enriched conditions in contrasting montane and lowland forests and assessed changes in the timing and magnitude of soil N-oxide emissions. We evaluated transitory effects, which occurred immediately after N addition, and long-term effects measured at least 6 weeks after N addition. In the montane forest where stem growth was N limited, the first-time N additions caused rapid increases in soil N-oxide emissions. During the first 2 years of N addition, annual N-oxide emissions were five times (transitory effect) and two times (long-term effect) larger than controls. This contradicts the current assumption that N-limited tropical montane forests will respond to N additions with only small and delayed increases in soil N-oxide emissions. We attribute this fast and large response of soil N-oxide emissions to the presence of an organic layer (a characteristic feature of this forest type) in which nitrification increased substantially following N addition. In the lowland forest where stem growth was neither N nor phosphorus (P) limited, the first-time N additions caused only gradual and minimal increases in soil N-oxide emissions. These first N additions were completed at the beginning of the wet season, and low soil water content may have limited nitrification. In contrast, the 9- and 10-year N-addition plots displayed instantaneous and large soil N-oxide emissions. Annual N-oxide emissions under chronic N addition were seven times (transitory effect) and four times (long-term effect) larger than controls. Seasonal changes in soil water content also caused seasonal changes in soil N-oxide emissions from the 9- and 10-year N-addition plots. This suggests that climate change scenarios, where rainfall quantity and seasonality change, will alter the relative importance of soil NO and N2O emissions from tropical forests exposed to elevated N deposition.
C1 [Koehler, Birgit; Corre, Marife D.; Veldkamp, Edzo; Wullaert, Hans] Univ Gottingen, Buesgen Inst Soil Sci Trop & Subtrop Ecosyst, Gottingen, Germany.
[Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama.
RP Corre, MD (reprint author), Univ Gottingen, Buesgen Inst Soil Sci Trop & Subtrop Ecosyst, Gottingen, Germany.
EM mcorre@gwdg.de
RI Veldkamp, Edzo/A-6660-2008; Wright, Stuart/M-3311-2013
OI Wright, Stuart/0000-0003-4260-5676
FU Robert Bosch Foundation (Germany)
FX We wish to thank Jim Dalling for his help during the selection of the
montane forest site; Rodolfo Rojas, Carlos Sanchez, Ignacio Delcid,
Olivier Gonzalez, Omar Hernandez and Rufino Gonzalez for their dedicated
assistance during field measurements; Norman Loftfield, Milton Garcia
and Jaime Florez for their help with the equipment; the Smithsonian
Tropical Research Institute for extending excellent logistical and
technical support; the laboratory staff of the Buesgen Institute,
University of Goettingen, for their assistance in laboratory analyses;
and two anonymous reviewers and M. Francesca Cotrufo for their positive
reviews. This study is under the NITROF project funded by the Robert
Bosch Foundation (Germany) and awarded to M. D. Corre as independent
research group leader.
NR 63
TC 54
Z9 57
U1 3
U2 56
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD AUG
PY 2009
VL 15
IS 8
BP 2049
EP 2066
DI 10.1111/j.1365-2486.2008.01826.x
PG 18
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 466XL
UT WOS:000267698400015
ER
PT J
AU Breitburg, DL
Craig, JK
Fulford, RS
Rose, KA
Boynton, WR
Brady, DC
Ciotti, BJ
Diaz, RJ
Friedland, KD
Hagy, JD
Hart, DR
Hines, AH
Houde, ED
Kolesar, SE
Nixon, SW
Rice, JA
Secor, DH
Targett, TE
AF Breitburg, D. L.
Craig, J. K.
Fulford, R. S.
Rose, K. A.
Boynton, W. R.
Brady, D. C.
Ciotti, B. J.
Diaz, R. J.
Friedland, K. D.
Hagy, J. D., III
Hart, D. R.
Hines, A. H.
Houde, E. D.
Kolesar, S. E.
Nixon, S. W.
Rice, J. A.
Secor, D. H.
Targett, T. E.
TI Nutrient enrichment and fisheries exploitation: interactive effects on
estuarine living resources and their management
SO HYDROBIOLOGIA
LA English
DT Article; Proceedings Paper
CT 2nd International Symposium on Research and Management of Eutrophication
in Coastal Ecosystems
CY JUN 20-23, 2006
CL Nyborg, DENMARK
DE Eutrophication; Hypoxia; Fisheries; Estuary; Management
ID GULF-OF-MEXICO; LOBSTER NEPHROPS-NORVEGICUS; CHESAPEAKE BAY; MARINE
ECOSYSTEMS; EPISODIC HYPOXIA; WATER-QUALITY; BALTIC COD; FOOD WEBS;
BEHAVIORAL-RESPONSES; COASTAL ECOSYSTEMS
AB Both fisheries exploitation and increased nutrient loadings strongly affect fish and shellfish abundance and production in estuaries. These stressors do not act independently; instead, they jointly influence food webs, and each affects the sensitivity of species and ecosystems to the other. Nutrient enrichment and the habitat degradation it sometimes causes can affect sustainable yields of fisheries, and fisheries exploitation can affect the ability of estuarine systems to process nutrients. The total biomass of fisheries landings in estuaries and semi-enclosed seas tends to increase with nitrogen loadings in spite of hypoxia, but hypoxia and other negative effects of nutrient over-enrichment cause declines in individual species and in parts of systems most severely affected. More thoroughly integrated management of nutrients and fisheries will permit more effective management responses to systems affected by both stressors, including the application of fisheries regulations to rebuild stocks negatively affected by eutrophication. Reducing fishing mortality may lead to the recovery of depressed populations even when eutrophication contributes to population declines if actions are taken while the population retains sufficient reproductive potential. New advances in modeling, statistics, and technology promise to provide the information needed to improve the understanding and management of systems subject to both nutrient enrichment and fisheries exploitation.
C1 [Breitburg, D. L.; Fulford, R. S.; Hines, A. H.; Kolesar, S. E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Craig, J. K.] N Carolina State Univ, Morehead City, NC 28557 USA.
[Craig, J. K.] Florida State Univ, Coastal & Marine Lab, St Teresa, FL 32358 USA.
[Fulford, R. S.] Univ So Mississippi, Dept Coastal Sci, Gulf Coast Res Lab, Ocean Springs, MS 39566 USA.
[Rose, K. A.] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA.
[Boynton, W. R.; Houde, E. D.; Secor, D. H.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA.
[Brady, D. C.; Ciotti, B. J.; Targett, T. E.] Univ Delaware, Coll Marine & Earth Studies, Lewes, DE 19958 USA.
[Diaz, R. J.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
[Friedland, K. D.] Natl Marine Fisheries Serv, Narragansett, RI 02882 USA.
[Hagy, J. D., III] US EPA, Natl Hlth & Environm Effects Res Lab, Gulf Ecol Div, Gulf Breeze, FL 32561 USA.
[Hart, D. R.] Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Woods Hole, MA 02543 USA.
[Kolesar, S. E.] St Marys Coll Maryland, St Marys City, MD 20686 USA.
[Nixon, S. W.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Rice, J. A.] N Carolina State Univ, Dept Biol, Raleigh, NC 27695 USA.
RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM breitburgd@si.edu
RI Boynton, Walter/C-3035-2012; Houde, Edward/D-8498-2012; Secor,
D/D-4367-2012; Ross, Donald/F-7607-2012
OI Secor, D/0000-0001-6007-4827; Ross, Donald/0000-0002-8659-3833
NR 112
TC 42
Z9 43
U1 6
U2 55
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0018-8158
J9 HYDROBIOLOGIA
JI Hydrobiologia
PD AUG
PY 2009
VL 629
IS 1
BP 31
EP 47
DI 10.1007/s10750-009-9762-4
PG 17
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 458NI
UT WOS:000267030400004
ER
PT J
AU Zimmermann, Y
Roubik, DW
Quezada-Euan, JJG
Paxton, RJ
Eltz, T
AF Zimmermann, Y.
Roubik, D. W.
Quezada-Euan, J. J. G.
Paxton, R. J.
Eltz, T.
TI Single mating in orchid bees (Euglossa, Apinae): implications for mate
choice and social evolution
SO INSECTES SOCIAUX
LA English
DT Article
DE Euglossini; Mating frequency; Mate choice; Microsatellites; Sociality;
Corbiculate bees
ID NESTING BIOLOGY; APIS-MELLIFERA; KIN SELECTION; HYMENOPTERA; APIDAE;
BEHAVIOR; FRAGRANCES; HONEYBEE; ACCUMULATION; COLLECTION
AB Neotropical orchid bees (Euglossini) are conspicuously different from other corbiculate bees (Apinae) in their lack of advanced sociality and in male use of acquired odors (fragrances) as pheromone-analogues. In both contexts, orchid bee mating systems, in particular the number of males a female mates with, are of great interest but are currently unknown. To assess female mating frequency in the genus Euglossa, we obtained nests from three species in Mexico and Panama and genotyped mothers and their brood at microsatellite DNA loci. In 26 out of 29 nests, genotypes of female brood were fully consistent with being descended from a singly mated mother. In nests with more than one adult female present, those adult females were frequently related, with genotypes being consistent with full sister-sister (r = 0.75) or mother-daughter (r = 0.5) relationships. Thus, our genetic data support the notions of female philopatry and nest-reuse in the genus Euglossa. Theoretically, single mating should promote the evolution of eusociality by maximizing the relatedness among individuals in a nest. However, in Euglossini this genetic incentive has not led to the formation of eusocial colonies as in other corbiculate bees, presumably due to differing ecological or physiological selective regimes. Finally, monandry in orchid bees is in agreement with the theory that females select a single best mate based on the male fragrance phenotype, which may contain information on male age, cognitive ability, and competitive strength.
C1 [Roubik, D. W.] Smithsonian Trop Res Inst, Balboa, Panama.
[Quezada-Euan, J. J. G.] Univ Autonoma Yucatan, Dept Apicultura, Merida, Mexico.
[Paxton, R. J.] Queens Univ Belfast, Sch Biol Sci, Belfast, Antrim, North Ireland.
[Zimmermann, Y.] Univ Dusseldorf, Dept Neurobiol, D-40225 Dusseldorf, Germany.
RP Zimmermann, Y (reprint author), Univ Dusseldorf, Inst Neurobiol, Univ Str 1, D-40225 Dusseldorf, Germany.
EM yvonne.zimmermann@uni-duesseldorf.de
RI Paxton, Robert/D-7082-2015
OI Paxton, Robert/0000-0003-2517-1351
FU Deutsche Forschungsgemeinschaft [EL 249/3]
FX We thank Tobias Wiesenfahrt for providing a Macintosh Computer and
Manuel Breuer for supporting the literature search. Klaus Lunau and the
members of the Sensory Ecology Group in Dusseldorf helped to improve the
manuscript; Martin Hasselmann patiently answered methodological
questions. Funding was provided to T. E. by the Deutsche
Forschungsgemeinschaft (DFG, EL 249/3).
NR 55
TC 14
Z9 14
U1 2
U2 19
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0020-1812
J9 INSECT SOC
JI Insect. Soc.
PD AUG
PY 2009
VL 56
IS 3
BP 241
EP 249
DI 10.1007/s00040-009-0017-1
PG 9
WC Entomology
SC Entomology
GA 472AX
UT WOS:000268102600003
ER
PT J
AU Boyle, SA
Lourenco, WC
da Silva, LR
Smith, AT
AF Boyle, Sarah A.
Lourenco, Waldete C.
da Silva, Livia R.
Smith, Andrew T.
TI Travel and Spatial Patterns Change When Chiropotes satanas chiropotes
Inhabit Forest Fragments
SO INTERNATIONAL JOURNAL OF PRIMATOLOGY
LA English
DT Article
DE Amazon; Brazil; conservation; deforestation; home range
ID HOME-RANGE SIZE; HABITAT USE; PROPITHECUS-DIADEMA; SPIDER MONKEYS; LOS
TUXTLAS; BODY-SIZE; PRIMATES; DIET; CONSERVATION; AREA
AB Previous studies have used home range size to predict a species' vulnerability to forest fragmentation. Northern bearded saki monkeys (Chiropotes satanas chiropotes) are medium-bodied frugivores with large home ranges, but sometimes they reside in forest fragments that are smaller than the species' characteristic home range size. Here we examine how travel and spatial patterns differ among groups living in forest fragments of 3 size classes (1 ha, 10 ha, and 100 ha) versus continuous forest. We collected data in 6 research cycles from July-August 2003 and January 2005-June 2006 at the Biological Dynamics of Forest Fragments Project (BDFFP), north of Manaus, Brazil. For each cycle, we followed the monkeys at each study site from dawn until dusk for 3 consecutive days, and recorded their location. Although bearded saki monkeys living in 10-ha and 1-ha fragments had smaller day ranges and traveled shorter daily distances, they traveled greater distances than expected based on the size of the forest fragment. Monkeys in the small fragments revisited a greater percentage of feeding trees each day, traveled in more circular patterns, and used the fragments in a more uniform pattern than monkeys in the continuous forest. Our results suggest that monkeys in the small fragments maximize their use of the forest, and that the preservation of large tracts of forest is essential for species conservation. Species with large home ranges sometimes inhabit forest fragments, but doing so can alter behavior, demographics, and ecology, and the monkeys may be vulnerable to stochastic events.
C1 [Boyle, Sarah A.; Lourenco, Waldete C.; da Silva, Livia R.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
[Boyle, Sarah A.; Lourenco, Waldete C.; da Silva, Livia R.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil.
[Boyle, Sarah A.; Smith, Andrew T.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
RP Boyle, SA (reprint author), Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
EM sarahannboyle@gmail.com
FU Brazil's National Counsel of Technological and Scientific Development;
Brazilian Institute of Environment and Renewable Natural Resources;
National Institute for Amazonian Research
FX We thank Brazil's National Counsel of Technological and Scientific
Development (Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico - CNPq), the Brazilian Institute of Environment and
Renewable Natural Resources (Instituto Brasileiro do Meio Ambiente e dos
Recursos Naturais Renovaveis - IBAMA), and the National Institute for
Amazonian Research (Instituto Nacional de Pesquisas da Amazonia - INPA)
for support and permission to conduct this research in Brazil. The
Biological Dynamics of Forest Fragments Project (BDFFP), Smithsonian
Tropical Research Institute, and Arizona State University provided
further logistical and financial support. This research was supported by
grants and fellowships to SB from Fulbright/Institute of International
Education, Margot Marsh Biodiversity Foundation, Providing Educational
Opportunities (PEO), Primate Conservation, Inc., Organization for
Tropical Studies, American Society of Primatologists, and IDEAWILD.
NR 77
TC 21
Z9 22
U1 2
U2 21
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0164-0291
EI 1573-8604
J9 INT J PRIMATOL
JI Int. J. Primatol.
PD AUG
PY 2009
VL 30
IS 4
BP 515
EP 531
DI 10.1007/s10764-009-9357-y
PG 17
WC Zoology
SC Zoology
GA 475MA
UT WOS:000268362400001
ER
PT J
AU Munoz-Fuentes, V
Darimont, CT
Wayne, RK
Paquet, PC
Leonard, JA
AF Munoz-Fuentes, Violeta
Darimont, Chris T.
Wayne, Robert K.
Paquet, Paul C.
Leonard, Jennifer A.
TI Ecological factors drive differentiation in wolves from British Columbia
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE Canis lupus; conservation biogeography; ESU; faecal DNA; GPS; landscape
genetics; mitochondrial DNA; museum specimens; phylogeography; wolf
ID WOLF CANIS-LUPUS; SALMON POISONING DISEASE; FALSE DISCOVERY RATE;
MITOCHONDRIAL-DNA; GENETIC-STRUCTURE; GRAY WOLF; ALEXANDER ARCHIPELAGO;
POPULATION DIFFERENTIATION; REPRODUCTIVE ISOLATION; SOUTHEASTERN ALASKA
AB Aim
Limited population structure is predicted for vagile, generalist species, such as the grey wolf (Canis lupus L.). Our aims were to study how genetic variability of grey wolves was distributed in an area comprising different habitats that lay within the potential dispersal range of an individual and to make inferences about the impact of ecology on population structure.
Location
British Columbia, Canada - which is characterized by a continuum of biogeoclimatic zones across which grey wolves are distributed - and adjacent areas in both Canada and Alaska, United States.
Methods
We obtained mitochondrial DNA control region sequences from grey wolves from across the province and integrated our genetic results with data on phenotype, behaviour and ecology (distance, habitat and prey composition). We also compared the genetic diversity and differentiation of British Columbia grey wolves with those of other North American wolf populations.
Results
We found strong genetic differentiation between adjacent populations of grey wolves from coastal and inland British Columbia. We show that the most likely factor explaining this differentiation is habitat discontinuity between the coastal and interior regions of British Columbia, as opposed to geographic distance or physical barriers to dispersal. We hypothesize that dispersing grey wolves select habitats similar to the one in which they were reared, and that this differentiation is maintained largely through behavioural mechanisms.
Main conclusions
The identification of strong genetic structure on a scale within the dispersing capabilities of an individual suggests that ecological factors are driving wolf differentiation in British Columbia. Coastal wolves are highly distinct and representative of a unique ecosystem, whereas inland British Columbia grey wolves are more similar to adjacent populations of wolves located in Alaska, Alberta and Northwest Territories. Given their unique ecological, morphological, behavioural and genetic characteristics, grey wolves of coastal British Columbia should be considered an Evolutionary Significant Unit (ESU) and, consequently, warrant special conservation status. If ecology can drive differentiation in a highly mobile generalist such as the grey wolf, ecology probably drives differentiation in many other species as well.
C1 [Munoz-Fuentes, Violeta; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, SE-75236 Uppsala, Sweden.
[Darimont, Chris T.] Univ Victoria, Dept Biol, Victoria, BC V8W 2Y2, Canada.
[Darimont, Chris T.] Raincoast Conservat Fdn, Denny Isl, BC, Canada.
[Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
[Paquet, Paul C.] Univ Calgary, Fac Environm Design, Calgary, AB T2N 1N4, Canada.
[Leonard, Jennifer A.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
RP Munoz-Fuentes, V (reprint author), Uppsala Univ, Dept Evolutionary Biol, SE-75236 Uppsala, Sweden.
EM violeta.munoz@ebc.uu.se
RI Munoz-Fuentes, Violeta/E-4218-2014; CSIC, EBD Donana/C-4157-2011;
Leonard, Jennifer/A-7894-2010
OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard,
Jennifer/0000-0003-0291-7819
FU Carl Trygger Foundation; National Geographic Society, Patagonia; Spanish
Ministry of Education; Swedish Research Council; US National Science
Foundation; Wilburforce Foundation; World Wildlife Fund Canada;
Raincoast Conservation Foundation; Rainforest Wolf Project
FX Randy Kadatz and Curtis English from the Alberta Environment Natural
Resources Service, Canada, assisted in sample collection. Adrian Walton
of the British Columbia Ministry of Forests provided the biogeoclimatic
data. We thank Helen Schwantje of the BC Ministry of Environment, Rex
Kenner from the University of British Columbia Cowan Vertebrate Museum,
Jim Cosgrove from the Royal British Columbia Museum, and the University
of Alaska for access to samples in collections. We thank Katrina Bennett
for her invaluable assistance with map production and Carles Vil for his
critical reading of the manuscript. Logistical support was provided by
the Center for Conservation & Evolutionary Genetics, National Zoological
Park, Smithsonian Institution, USA. Funding was provided by the Carl
Trygger Foundation, the National Geographic Society, Patagonia, the
Spanish Ministry of Education, the Swedish Research Council, the US
National Science Foundation, the Wilburforce Foundation and the World
Wildlife Fund Canada. We thank the Raincoast Conservation Foundation for
initiating and supporting the Rainforest Wolf Project, as well as for
funding a portion of this work. Field sampling occurred in the
Traditional Territories of several First Nation groups, from whom we
obtained permission before research began. In particular, we thank the
Heiltsuk Nation, which has been a project partner since inception.
NR 96
TC 44
Z9 45
U1 7
U2 66
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD AUG
PY 2009
VL 36
IS 8
BP 1516
EP 1531
DI 10.1111/j.1365-2699.2008.02067.x
PG 16
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 471KH
UT WOS:000268056000009
ER
PT J
AU Parenti, LR
Viloria, AL
Ebach, MC
Morrone, JJ
AF Parenti, Lynne R.
Viloria, Angel L.
Ebach, Malte C.
Morrone, Juan J.
TI On the International Code of Area Nomenclature (ICAN): a reply to
Zaragueta-Bagils et al.
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Letter
DE Area classification; area names; area nomenclature; area ranks; ICAN;
standards in biogeography
ID FISHES
AB In 2007 the Systematic and Evolutionary Biogeographical Association (SEBA) wrote and ratified the first draft of the International Code of Area Nomenclature (ICAN), which was posted subsequently on the SEBA website. The ICAN was published, along with an explanatory discussion, by Ebach et al. (Journal of Biogeography, 35, 2008, 1153-1157), an article that is the subject of criticism by Zaragueta-Bagils et al. (Journal of Biogeography, 36, 2009, 1617-1618). We welcome discussion of the issues raised by these authors and respond to them briefly here. For many reasons, we reject the proposition that implementation of the ICAN be postponed until it is flawless. The ICAN has already been implemented. Further, it is the nature of nomenclatural codes to be proposed and then revised periodically to suit our applications. Most importantly, standardization of area names in biogeography is long overdue.
C1 [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Viloria, Angel L.] Inst Venezolano Invest Cient, Ctr Ecol, Caracas 1020A, Venezuela.
[Ebach, Malte C.] Arizona State Univ, Coll Liberal Arts & Sci, Int Inst Species Explorat, Tempe, AZ 85287 USA.
[Ebach, Malte C.] Arizona State Univ, Coll Liberal Arts & Sci, Sch Life Sci, Tempe, AZ 85287 USA.
[Morrone, Juan J.] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Evolut Biol, Museo Zool Alfonso L Herrera, Mexico City 04510, DF, Mexico.
RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012,MRC 159, Washington, DC 20013 USA.
EM parentil@si.edu
OI Morrone, Juan/0000-0001-5566-1189; Ebach, Malte/0000-0002-9594-9010
NR 15
TC 1
Z9 1
U1 0
U2 4
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD AUG
PY 2009
VL 36
IS 8
BP 1620
EP 1621
DI 10.1111/j.1365-2699.2009.02171.x
PG 2
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 471KH
UT WOS:000268056000020
ER
PT J
AU Eissler, Y
Wang, K
Chen, F
Wommack, KE
Coats, DW
AF Eissler, Yoanna
Wang, Kui
Chen, Feng
Wommack, K. Eric
Coats, D. Wayne
TI ULTRASTRUCTURAL CHARACTERIZATION OF THE LYTIC CYCLE OF AN INTRANUCLEAR
VIRUS INFECTING THE DIATOM CHAETOCEROS CF. WIGHAMII(BACILLARIOPHYCEAE)
FROM CHESAPEAKE BAY, USA
SO JOURNAL OF PHYCOLOGY
LA English
DT Article
DE algal virus; Chaetoceros; diatom; viral ecology; virus
ID HETEROSIGMA-AKASHIWO RAPHIDOPHYCEAE; PHYTOPLANKTON COMPOSITION;
RHIZOSOLENIA-SETIGERA; VIRAL MORTALITY; MARINE VIRUSES; RED TIDE;
PARTICLES; LYSIS; SIZE; BIOAVAILABILITY
AB Numerous microalgal species are infected by viruses that have the potential to control phytoplankton dynamics by reducing host populations, preventing bloom formation, or causing the collapse of blooms. Here we describe a virus infecting the diatom Chaetoceros cf. wighamii Brightw. from the Chesapeake Bay. To characterize the morphology and lytic cycle of this virus, we conducted a time-course experiment, sampling every 4 h over 72 h following viral inoculation. In vivo fluorescence began to decline 16 h after inoculation and was reduced to < 19% of control cultures by the end of experiment. TEM confirmed infection within the first 8 h of inoculation, as indicated by the presence of virus-like particles (VLP) in the nuclei. VLP were present in two different arrangements: rod-like structures that appeared in cross-section as paracrystalline arrays of hexagonal-shaped profiles measuring 12 +/- 2 nm in diameter and uniformly electron-dense hexagonal-shaped particles measuring similar to 22-28 nm in diameter. Nuclei containing paracrystalline arrays were most prevalent early in the infection cycle, while cells containing VLP increased and then declined toward the end of the cycle. The proportion of nuclei containing both paracrystalline arrays and VLP remained relatively constant. This pattern suggests that rod-like paracrystalline arrays fragmented to produce icosahedral VLP. C. cf. wighamii nuclear inclusion virus (CwNIV) is characterized by a high burst size (averaged 26,400 viruses per infected cell) and fast generation time that could have ecological implications on C. cf. wighamii population control.
C1 [Eissler, Yoanna] Univ Valparaiso, Ctr Invest & Gest Recursos Nat, Dept Quim & Bioquim, Fac Ciencias, Valparaiso, Chile.
[Eissler, Yoanna] Univ Austral Chile, CIEN Austral, Puerto Montt, Chile.
[Wang, Kui; Chen, Feng] Univ Maryland, Ctr Marine Biotechnol, Baltimore, MD 21202 USA.
[Wommack, K. Eric] Delaware Biotechnol Inst, Newark, DE 19711 USA.
[Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Eissler, Y (reprint author), Univ Valparaiso, Ctr Invest & Gest Recursos Nat, Dept Quim & Bioquim, Fac Ciencias, Gran Bretana 1111, Valparaiso, Chile.
EM yoanna.eissler@uv.cl
RI Chen, Feng/P-3088-2014
FU National Science Foundation [MCB-0132070]
FX We thank Drs. Richard V. Lacouture and Marie Anne Hartsig for their help
in identification of Chaetoceros species and for providing microalgal
cultures. We are also grateful to Dr. Harold Marshall for providing SEM
images used in this study. This research was supported by National
Science Foundation grant MCB-0132070 to K. E. W., F. C., D. W. C.
NR 40
TC 15
Z9 18
U1 1
U2 8
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD AUG
PY 2009
VL 45
IS 4
BP 787
EP 797
DI 10.1111/j.1529-8817.2009.00705.x
PG 11
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 488TF
UT WOS:000269372300001
PM 27034207
ER
PT J
AU Aguilar, R
Johnson, EG
Hines, AH
Roberts, PM
Goodison, MR
Kramer, MA
AF Aguilar, Robert
Johnson, Eric G.
Hines, Anson H.
Roberts, Paige M.
Goodison, Michael R.
Kramer, Margaret A.
TI POPULATION AND FISHERY DYMANICS OF BLUE CRABS CALLINECTES SAPIDUS IN A
SUBESTUARY OF CHESAPEAKE BAY
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Aguilar, Robert; Johnson, Eric G.; Hines, Anson H.; Roberts, Paige M.; Goodison, Michael R.; Kramer, Margaret A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2009
VL 28
IS 3
BP 677
EP 677
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 546HK
UT WOS:000273801700068
ER
PT J
AU Johnson, E
Hines, A
Kramer, M
Goodison, M
Aguilar, R
Soulen, H
Roberts, P
Zohar, Y
Zmora, O
AF Johnson, Eric
Hines, Anson
Kramer, Margaret
Goodison, Michael
Aguilar, Robert
Soulen, Heather
Roberts, Paige
Zohar, Yonathan
Zmora, Oded
TI FIELD ASSESSMENT OF BLUE CRAB RESTOCKING IN UPPER CHESAPEAKE BAY
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Johnson, Eric; Hines, Anson; Kramer, Margaret; Goodison, Michael; Aguilar, Robert; Soulen, Heather; Roberts, Paige] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Zohar, Yonathan; Zmora, Oded] Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, Baltimore, MD 21202 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 2
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2009
VL 28
IS 3
BP 705
EP 706
PG 2
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 546HK
UT WOS:000273801700171
ER
PT J
AU Riley, S
AF Riley, Sheila
TI Mortal Friends
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC 20113 USA.
RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC 20113 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD AUG
PY 2009
VL 134
IS 13
BP 68
EP 68
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 488HR
UT WOS:000269340500074
ER
PT J
AU Guz, SS
AF Guz, Savannah Schroll
TI Vietnam War Era: People and Perspectives.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD AUG
PY 2009
VL 134
IS 13
BP 110
EP 110
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 488HR
UT WOS:000269340500295
ER
PT J
AU Simkanin, C
Davidson, I
Falkner, M
Sytsma, M
Ruiz, G
AF Simkanin, Christina
Davidson, Ian
Falkner, Maurya
Sytsma, Mark
Ruiz, Gregory
TI Intra-coastal ballast water flux and the potential for secondary spread
of non-native species on the US West Coast
SO MARINE POLLUTION BULLETIN
LA English
DT Article
DE Aquatic non-native species; Ballast water; Commercial shipping; Domestic
shipping; Intra-coastal transport; Secondary spread
ID MARINE BIOLOGICAL INVASIONS; LAURENTIAN GREAT-LAKES; GENETIC DIVERSITY;
PACIFIC-OCEAN; UNITED-STATES; MITTEN CRAB; PATTERNS; ORGANISMS; VECTOR;
SHIPS
AB Ballast water is a dominant mechanism for the interoceanic and transoceanic dispersal of aquatic nonnative species (ANS), but few studies have addressed ANS transfers via smaller scale vessel movements. We analyzed ballast water reporting records and ANS occurrence data from four US West Coast port systems to examine patterns of intra-coastal ballast water transfer, and assess how ballast transfers may have influenced the secondary spread of ANS. In 2005, one third of the vessels arriving to the US West Coast originated at one of four West Coast port systems (intra-coastal traffic). These vessels transported and discharged 27% (5,987,588 MT) of the total ballast water volume discharged at these ports that year. The overlap of ANS (shared species) among port systems varied between 3% and 80%, with the largest overlap occurring between San Francisco Bay and LA/Long Beach. Our results suggest that intra-coastal ballast water needs further consideration as an invasion pathway, especially as efforts to promote short-sea shipping are being developed. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Simkanin, Christina; Davidson, Ian; Sytsma, Mark; Ruiz, Gregory] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA.
[Falkner, Maurya] Calif State Lands Commiss, Marine Facil Div, Sacramento, CA 95825 USA.
[Ruiz, Gregory] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Simkanin, C (reprint author), Univ Victoria, Dept Biol, POB 3020 STN CSC, Victoria, BC V8W 3N5, Canada.
EM simkanin@uvic.ca
RI Sytsma, Mark/B-2746-2013;
OI Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048
FU Pacific States Marine Fisheries Commission; National Oceanic and
Atmospheric Administration
FX We are grateful to Pamala Meacham and Allen Pleus at the Washington
Department of Fish and Wildlife for providing access to Washington State
ballast water reporting records. We thank Dr. Paul Fofonoff at the
Smithsonian Environmental Research Center for providing insight and
access to the National Exotic Marine and Estuarine Species Information
System (NEMESIS). We are also grateful to Nicole Dobroski and Chris
Scianni for helpful comments on the manuscript, and Vanessa Howard for
creating Fig. 1. We gratefully acknowledge funding support from the
Pacific States Marine Fisheries Commission and the National Oceanic and
Atmospheric Administration. This study is dedicated to Patricia Moran
Simkanin.
NR 53
TC 38
Z9 40
U1 1
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0025-326X
EI 1879-3363
J9 MAR POLLUT BULL
JI Mar. Pollut. Bull.
PD AUG
PY 2009
VL 58
IS 3
BP 366
EP 374
DI 10.1016/j.marpolbul.2008.10.013
PG 9
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 425QT
UT WOS:000264652900017
PM 19108853
ER
PT J
AU Mair, JM
Cunningham, SL
Sibaja-Cordero, JA
Guzman, HM
Arroyo, MF
Merino, D
Vargas, R
AF Mair, James M.
Cunningham, Sarah L.
Sibaja-Cordero, Jeffrey A.
Guzman, Hector M.
Fernanda Arroyo, Maria
Merino, Daisi
Vargas, Rita
TI Mapping benthic faunal communities in the shallow and deep sediments of
Las Perlas Archipelago, Pacific Panama
SO MARINE POLLUTION BULLETIN
LA English
DT Article
DE Pacific Panama; Sediment; Benthic invertebrate communities; MPA
ID COIBA-NATIONAL-PARK; POPULATION ASSESSMENT; COSTA-RICA; MARINE; SEA;
POLYCHAETA; DIVERSITY; SYLLIDAE; SHELF; REEF
AB Las Perlas Archipelago (LPA) is located off the Pacific Coast of Panama and was designated as a marine protected area (MPA) in 2007. This baseline study of the shallow and deeper sedimentary habitats of the islands partly informed the MPA designation. Ninety-two grab stations and twenty trawl stations were sampled. Sediment grab sample results were interpolated to produce a map that showed the area to be dominated by mud (1246 km(2), 40%) and sand/shell sediments (780 km(2), 25%). A total of 201 taxa were recorded and over 5800 individual specimens were processed, revealing that the sediments hold varying community compositions, with annelids being the dominant group (73%) followed by crustaceans (14%). Relationships were evident between community, feeding guilds, and sediment types, which give an indication of communities that can be expected in similar sediments in other areas of the Tropical Eastern Pacific. A study of this scale and level of detail is rare for this biogeographic region and provides a valuable, comprehensive appreciation of the LPA's benthos. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Mair, James M.] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland.
[Cunningham, Sarah L.] Argyll & Bute Council, Marine & Coastal Dev Unit, Oban PA34 4LF, Argyll, Scotland.
[Sibaja-Cordero, Jeffrey A.] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 2060, Costa Rica.
[Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Fernanda Arroyo, Maria; Merino, Daisi] Univ Guayaquil, Fac Ciencias Nat, Guayaquil, Ecuador.
[Vargas, Rita] Univ Costa Rica, Museo Zool, Escuela Biol, San Jose 2060, Costa Rica.
RP Mair, JM (reprint author), Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland.
EM j.m.mair@hw.ac.uk
FU UK government's Department for Environment, Food and Rural Affairs
(DEFRA), Heriot-Watt University, UK; Smithsonian Tropical Research
Institute, Panama
FX We thank the Government of Panama for providing permits to work and
collect in the area. The authors would like to thank C. Guevara, J.M.
Guevara, B. Medina, L. Barrios, J. Berman, S. Chambers and the crew of
R/V Urraca who assisted during fieldwork. We thank H. Collazos for
invaluable support in analysing sediment samples. Funding for this study
was partially provided by the Darwin Initiative, a programme of the UK
government's Department for Environment, Food and Rural Affairs (DEFRA),
Heriot-Watt University, UK and the Smithsonian Tropical Research
Institute, Panama.
NR 35
TC 9
Z9 11
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0025-326X
EI 1879-3363
J9 MAR POLLUT BULL
JI Mar. Pollut. Bull.
PD AUG
PY 2009
VL 58
IS 3
BP 375
EP 383
DI 10.1016/j.marpolbul.2008.10.015
PG 9
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 425QT
UT WOS:000264652900018
PM 19081116
ER
PT J
AU Cheimets, P
Gordon, J
Tull, J
AF Cheimets, Peter
Gordon, Joshua
Tull, James
TI Product development today is often about teamwork, and there are
teachable skills to give engineers more influence in group decisions.
SO MECHANICAL ENGINEERING
LA English
DT Article
C1 [Cheimets, Peter] Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Cheimets, P (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA.
NR 0
TC 1
Z9 1
U1 1
U2 1
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0025-6501
J9 MECH ENG
JI Mech. Eng.
PD AUG
PY 2009
VL 131
IS 8
BP 26
EP 29
PG 4
WC Engineering, Mechanical
SC Engineering
GA 616ZX
UT WOS:000279251600020
ER
PT J
AU Plotkin, H
Clarke, RS
AF Plotkin, H.
Clarke, R. S., Jr.
TI Stuart H. Perry's contributions to meteorite collection and research,
1927-1957
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
AB Stuart H. Perry (1874-1957), an influential Michigan newspaper editor and publisher and a vice president of the Associated Press, developed a passionate interest in collecting and Studying meteorites in the 1920s and 1930s. Firmly believing that meteorites belong in great museums where they call be properly investigated, lie generously donated his meteorites to various museums after lie finished his Own Study of them. He had a sincere interest in the National Collection of Meteorites, and donated 192 specimens-mostly irons-to the U.S. National Museum; these Constituted some of the most important meteorites in its collection, and moved iron meteorites to center stage, a position still occupied. By applying Current metallographic methods to the study of iron meteorites, Perry directed scientists to a powerful new research tool, which led to major advances in our understanding of meteoritic irons and helped give rise to a new field within planetary sciences. His groundbreaking monograph The metallography of meteoric iron served as a standard reference collection of metallographic photomicrographs of iron meteorites for more than 30 years. It remained ail insightful and useful work on the structure of meteoritic iron until improved binary and tertiary phase diagrams in the Fe-Ni(-P) system allowed a more detailed treatment of the formation of iron meteorites. Perry received many honors for his work, and held office in the Meteoritical Society, serving as a councilor from 1941-1950, and as a vice president from 1950-1957.
C1 [Plotkin, H.] Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada.
[Clarke, R. S., Jr.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Plotkin, H (reprint author), Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada.
EM hplotkin@rogers.com
FU Edward P. and Rebecca Rogers Henderson Fund
FX The authors thank MAPS reviewers Drs. Derek Sears and Stephen Kissin and
associate editor Dr. Ed Scott for their helpful reviews. We also thank
Dr. Ursula Marvin, Center for Astrophysics, Smithsonian Astrophysical
Observatory, for her helpful comments on ail earlier draft of the
manuscript. As well, we acknowledge the debt we owe to Dr. Timothy
McCoy, National Museum of Natural History, Smithsonian Institution,
whose incisive comments and help proved crucial to the completion of the
final draft. Lastly, we thank LuElla Speakman and Dr. Cari Corrigan,
also of the National Museum of Natural History, for their help in the
technical production of the manuscript. We are grateful to the Edward P.
and Rebecca Rogers Henderson Fund for Supporting this research.
NR 53
TC 1
Z9 1
U1 0
U2 0
PU METEORITICAL SOC
PI FAYETTEVILLE
PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2009
VL 44
IS 8
BP 1161
EP 1177
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 515BX
UT WOS:000271442600007
ER
PT J
AU Fierer, N
Carney, KM
Horner-Devine, MC
Megonigal, JP
AF Fierer, Noah
Carney, Karen M.
Horner-Devine, M. Claire
Megonigal, J. Patrick
TI The Biogeography of Ammonia-Oxidizing Bacterial Communities in Soil
SO MICROBIAL ECOLOGY
LA English
DT Article
ID 16S RIBOSOMAL-RNA; GRADIENT GEL-ELECTROPHORESIS; NITROGEN
MINERALIZATION; MICROBIAL BIOGEOGRAPHY; PHYLOGENETIC DIVERSITY;
MANAGEMENT REGIMENS; MOLECULAR ANALYSIS; CASCADE MOUNTAINS;
SPECIES-DIVERSITY; FOREST SOILS
AB Although ammonia-oxidizing bacteria (AOB) are likely to play a key role in the soil nitrogen cycle, we have only a limited understanding of how the diversity and composition of soil AOB communities change across ecosystem types. We examined 23 soils collected from across North America and used sequence-based analyses to compare the AOB communities in each of the distinct soils. Using 97% 16S rRNA sequence similarity groups, we identified only 24 unique AOB phylotypes across all of the soils sampled. The majority of the sequences collected were in the Nitrosospira lineages (representing 80% of all the sequences collected), and AOB belonging to Nitrosospira cluster 3 were particularly common in our clone libraries and ubiquitous across the soil types. Community composition was highly variable across the collected soils, and similar ecosystem types did not always harbor similar AOB communities. We did not find any significant correlations between AOB community composition and measures of N availability. From the suite of environmental variables measured, we found the strongest correlation between temperature and AOB community composition; soils exposed to similar mean annual temperatures tended to have similar AOB communities. This finding is consistent with previous studies and suggests that temperature selects for specific AOB lineages. Given that distinct AOB taxa are likely to have unique functional attributes, the biogeographical patterns exhibited by soil AOB may be directly relevant to understanding soil nitrogen dynamics under changing environmental conditions.
C1 [Fierer, Noah] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Fierer, Noah] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Carney, Karen M.] Stratus Consulting Inc, Washington, DC 20036 USA.
[Horner-Devine, M. Claire] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.
[Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Fierer, N (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, CIRES UCB 216, Boulder, CO 80309 USA.
EM noah.fierer@colorado.edu
FU National Science Foundation [MCB 0610970, DEB 0516400]; Andrew W. Mellon
Foundation; Smithsonian Institution Fellowship
FX We thank the many individuals who donated their time and resources to
help with soil collection. We particularly want to thank Ben Colman for
his help with the soil analyses. In addition, both Josh Schimel and Rob
Jackson provided valuable logistical and intellectual support for this
project. Four anonymous reviewers provided very useful comments on a
previous draft of this manuscript. This work was supported by grants
awarded to N. F. from the National Science Foundation (MCB 0610970) and
the Andrew W. Mellon Foundation, a Smithsonian Institution Fellowship to
K. C., and a National Science Foundation grant (DEB 0516400) to P. M.
NR 51
TC 61
Z9 68
U1 2
U2 44
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
J9 MICROB ECOL
JI Microb. Ecol.
PD AUG
PY 2009
VL 58
IS 2
BP 435
EP 445
DI 10.1007/s00248-009-9517-9
PG 11
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 470YS
UT WOS:000268019000018
PM 19352770
ER
PT J
AU Hopkins, PF
Somerville, RS
Cox, TJ
Hernquist, L
Jogee, S
Keres, D
Ma, CP
Robertson, B
Stewart, K
AF Hopkins, Philip F.
Somerville, Rachel S.
Cox, Thomas J.
Hernquist, Lars
Jogee, Shardha
Keres, Dusan
Ma, Chung-Pei
Robertson, Brant
Stewart, Kyle
TI The effects of gas on morphological transformation in mergers:
implications for bulge and disc demographics
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies:
spiral; cosmology: theory
ID STAR-FORMING GALAXIES; TULLY-FISHER RELATION; HUBBLE-SPACE-TELESCOPE;
COLD DARK-MATTER; ULTRALUMINOUS INFRARED GALAXIES; INTEGRAL-FIELD
SPECTROSCOPY; ANGULAR-MOMENTUM PROBLEM; ACTIVE GALACTIC NUCLEI;
GOODS-MUSIC SAMPLE; ULTRA-DEEP-FIELD
AB Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T similar to 0.5 at < 10(10) M(circle dot), with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T similar to 0.1 at < 10(10) M(circle dot), with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests.
C1 [Hopkins, Philip F.; Ma, Chung-Pei] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Somerville, Rachel S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Somerville, Rachel S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Cox, Thomas J.; Hernquist, Lars; Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jogee, Shardha] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Robertson, Brant] Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Robertson, Brant] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Stewart, Kyle] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM phopkins@astro.berkeley.edu
FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690]; NASA ATP
[NAG5-12140, NAG5-13292, NAG5-13381]; Harvard University
FX We thank Fabio Governato, James Bullock and Chris Purcell for helpful
discussions. We also thank the anonymous referee for suggestions that
improved this manuscript. This work was supported in part by NSF grants
ACI 96-19019, AST 00-71019, AST 02-06299 and AST 03-07690, and NASA ATP
grants NAG5-12140, NAG5-13292 and NAG5-13381. Support for PFH was
provided by the Miller Institute for Basic Research in Science,
University of California Berkeley. Support for TJC was provided by the
W. M. Keck Foundation. Support for DK was provided by Harvard University
and the Institute for Theory and Computation (ITC). RSS thanks the ITC
at Harvard University for supporting visits that contributed to this
work.
NR 162
TC 119
Z9 119
U1 0
U2 4
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 1
PY 2009
VL 397
IS 2
BP 802
EP 814
DI 10.1111/j.1365-2966.2009.14983.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 472AJ
UT WOS:000268100700018
ER
PT J
AU Werner, VR
Laughinghouse, HD
AF Werner, Vera Regina
Laughinghouse, Haywood Dail
TI Bloom-forming and other planktonic Anabaena (Cyanobacteria)
morphospecies with twisted trichomes from Rio Grande do Sul State,
Brazil
SO NOVA HEDWIGIA
LA English
DT Article
ID GENERA ANABAENA; GENUS ANABAENA; CYANOPROKARYOTES; APHANIZOMENON;
NOSTOCALES; STRAINS
AB Many planktonic Anabaena with twisted trichomes are morphologically similar leading to improper identification, especially as A. spiroides. However, many studies have shown differences among them, and several distinguishable species have been described. This study aimed at the taxonomic analysis of natural populations, contributing to the knowledge of the diversity and distribution of Anabaena in subtropical and temperate environments of southern Brazil. Based on the morphology of populations from different water bodies in Rio Grande do Sul State, emphasizing on those reported in blooms from reservoirs supplying public drinking water, nine taxa were recognized. Six morphospecies were forming blooms, among them, five were found toxic. Anabaena mucosa and A. nygaardii are reported for the first time in continental America and A. mendotae for South America. This study correctly identifies A. oumiana for the first time in South America with descriptions, illustrations, and comments. Descriptions, critical analyses of taxonomic features for specific delimitation, measurements, and illustrations of the taxa are presented. Since this study was based on morphology, we consider that further research will be carried out based on ultra-structure and genetic traits.
C1 [Werner, Vera Regina] Fundacao Zoobot Rio Grande Sul, Museu Ciencias Nat, BR-90001970 Porto Alegre, RS, Brazil.
Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA.
RP Werner, VR (reprint author), Fundacao Zoobot Rio Grande Sul, Museu Ciencias Nat, Caixa Postal 1188, BR-90001970 Porto Alegre, RS, Brazil.
EM vrwerner@fzb.rs.gov.br
RI Laughinghouse, Haywood/M-5836-2016
OI Laughinghouse, Haywood/0000-0003-1018-6948
FU CNPq [104716/2005-3]
FX Special thanks are given to Dr. Jiri Komarek and Dr. Masayuki Watanabe
for their valuable comments and information; to CNPq (PIBIC-MCN/FZBRS -
Grant 104716/2005-3) for financial support to the second author; to
colleagues from water/sewage treatment plants in Rio Grande do Sul
(CORSAN, DMAE, and SAMAE-Caxias do Sul) and from "Fundacao Universidade
Federal do Rio Grande" (FURG) for providing various studied samples; and
to Rejane Rosa and Everton Luis Luz de Quadros from MCN/FZBRS, for
passing Indian ink on the line drawings for final print and for
designing the maps, respectively.
NR 41
TC 8
Z9 8
U1 0
U2 1
PU GEBRUDER BORNTRAEGER
PI STUTTGART
PA JOHANNESSTR 3A, D-70176 STUTTGART, GERMANY
SN 0029-5035
J9 NOVA HEDWIGIA
JI Nova Hedwigia
PD AUG
PY 2009
VL 89
IS 1-2
BP 17
EP 47
DI 10.1127/0029-5035/2009/0089-0017
PG 31
WC Plant Sciences
SC Plant Sciences
GA 478VH
UT WOS:000268616100002
ER
PT J
AU Tardif, SD
Power, ML
Ross, CN
Rutherford, JN
Layne-Colon, DG
Paulik, MA
AF Tardif, Suzette D.
Power, Michael L.
Ross, Corinna N.
Rutherford, Julienne N.
Layne-Colon, Donna G.
Paulik, Mark A.
TI Characterization of Obese Phenotypes in a Small Nonhuman Primate, the
Common Marmoset (Callithrix jacchus)
SO OBESITY
LA English
DT Article
ID CHILDHOOD OBESITY; BODY-COMPOSITION; METABOLIC SYNDROME; RISK-FACTORS;
DIABETES-MELLITUS; MONKEYS; PREVALENCE; GROWTH; CHILDREN; WEIGHT
AB This report explores aspects of developing obesity in two captive populations of common marmosets (Callithrix jacchus), a small primate with a short lifespan that may be of value in modeling chronic aspects of obesity acquisition and its lifetime effects. Two populations were examined. In study 1, body composition, lipid parameters, and glucose metabolic parameters were measured in a population of 64 adult animals. Animals classified as obese (>80th percentile relative fat based on sex) displayed both dyslipidemia (higher triglyceride and very low-density lipoprotein (VLDL)) and altered glucose metabolism (higher fasting glucose and HbA(1c)). Using operational definitions of atypical values for factors associated with metabolic syndrome in humans, five subjects (7.8%) had at least three atypical factors and five others had two atypical factors. A previously unreported finding in these normally sexually monomorphic primates was higher body weight, fat weights, and percent fat in females compared to males. In a second study, longitudinal weight data for a larger population (n = 210) were analyzed to evaluate the development of high weight animals. Differences in weights for animals that would exceed the 90th percentile in early adulthood were evident from infancy, with a 15% difference in weight between future-large weight vs. their future-normal weight litter mates as early as 4-6 months of age. The marmoset, therefore, demonstrates similar suites of obesity-related alterations to those seen in other primates, including humans, suggesting that this species is worthy of consideration for obesity studies in which its fast maturity, high fertility, relatively short lifespan, and small size may be of advantage.
C1 [Tardif, Suzette D.; Ross, Corinna N.] Univ Texas Hlth Sci Ctr San Antonio, Barshop Inst Longev & Aging Studies, San Antonio, TX 78229 USA.
[Tardif, Suzette D.; Ross, Corinna N.; Layne-Colon, Donna G.] SW Natl Primate Res Ctr, San Antonio, TX USA.
[Power, Michael L.] Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA.
[Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Washington, DC 20024 USA.
[Rutherford, Julienne N.] Northwestern Univ, Dept Anthropol, Evanston, IL 60208 USA.
[Paulik, Mark A.] GlaxoSmithKline, Res Triangle Pk, NC USA.
RP Tardif, SD (reprint author), Univ Texas Hlth Sci Ctr San Antonio, Barshop Inst Longev & Aging Studies, San Antonio, TX 78229 USA.
EM tardif@uthscsa.edu
FU NIDDK NIH HHS [R01 DK077639]
NR 48
TC 34
Z9 34
U1 0
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1930-7381
EI 1930-739X
J9 OBESITY
JI Obesity
PD AUG
PY 2009
VL 17
IS 8
BP 1499
EP 1505
DI 10.1038/oby.2009.77
PG 7
WC Endocrinology & Metabolism; Nutrition & Dietetics
SC Endocrinology & Metabolism; Nutrition & Dietetics
GA 475QD
UT WOS:000268374200006
PM 19325546
ER
PT J
AU Cai, ZQ
Schnitzer, SA
Bongers, F
AF Cai, Zhi-Quan
Schnitzer, Stefan A.
Bongers, Frans
TI Seasonal differences in leaf-level physiology give lianas a competitive
advantage over trees in a tropical seasonal forest
SO OECOLOGIA
LA English
DT Article
DE Liana distribution; Nitrogen-use efficiency; Tropical forest physiology;
Water-use efficiency
ID BARRO-COLORADO ISLAND; RAIN-FOREST; EASTERN AMAZONIA; FUNCTIONAL-GROUPS;
SECONDARY FOREST; NITROGEN-CONTENT; CLIMBING PLANTS; ELEVATED CO2; MOIST
FOREST; DRY FOREST
AB Lianas are an important component of most tropical forests, where they vary in abundance from high in seasonal forests to low in aseasonal forests. We tested the hypothesis that the physiological ability of lianas to fix carbon (and thus grow) during seasonal drought may confer a distinct advantage in seasonal tropical forests, which may explain pan-tropical liana distributions. We compared a range of leaf-level physiological attributes of 18 co-occurring liana and 16 tree species during the wet and dry seasons in a tropical seasonal forest in Xishuangbanna, China. We found that, during the wet season, lianas had significantly higher CO(2) assimilation per unit mass (A (mass)), nitrogen concentration (N (mass)), and delta(13)C values, and lower leaf mass per unit area (LMA) than trees, indicating that lianas have higher assimilation rates per unit leaf mass and higher integrated water-use efficiency (WUE), but lower leaf structural investments. Seasonal variation in CO(2) assimilation per unit area (A (area)), phosphorus concentration per unit mass (P (mass)), and photosynthetic N-use efficiency (PNUE), however, was significantly lower in lianas than in trees. For instance, mean tree A (area) decreased by 30.1% from wet to dry season, compared with only 12.8% for lianas. In contrast, from the wet to dry season mean liana delta(13)C increased four times more than tree delta(13)C, with no reduction in PNUE, whereas trees had a significant reduction in PNUE. Lianas had higher A (mass) than trees throughout the year, regardless of season. Collectively, our findings indicate that lianas fix more carbon and use water and nitrogen more efficiently than trees, particularly during seasonal drought, which may confer a competitive advantage to lianas during the dry season, and thus may explain their high relative abundance in seasonal tropical forests.
C1 [Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA.
[Cai, Zhi-Quan] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Peoples R China.
[Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa 084303092, Panama.
[Cai, Zhi-Quan; Bongers, Frans] Univ Wageningen & Res Ctr, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, Wageningen, Netherlands.
RP Schnitzer, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA.
EM schnitzer@uwm.edu
OI Schnitzer, Stefan/0000-0002-2715-9455
FU National Science Foundation in China [NSFC-30500065]; Wageningen
University [sandwich-PhD grant]
FX We thank Chen YaJun and three undergraduate students from Simao Normal
College for help with the field work, and S. Mangan, J. Mascaro, L.
Poorter, H. Qinming, M. Tobin, and A. Wright for constructive comments.
Liu WenJie kindly provided meteorological data from the Ecological
Monitoring Station in XTBG. We also thank Li LeYi for carbon isotope
analyses, Fu Yun for nutrient analyses, and Wen Bin for species
identification. This work was supported financially by a grant
(NSFC-30500065) from the National Science Foundation in China, and by a
sandwich-PhD grant from Wageningen University. The experiments conducted
in this study comply with the current laws of China.
NR 60
TC 56
Z9 65
U1 5
U2 34
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD AUG
PY 2009
VL 161
IS 1
BP 25
EP 33
DI 10.1007/s00442-009-1355-4
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 462IT
UT WOS:000267345500003
PM 19418072
ER
PT J
AU Lasso, E
Engelbrecht, BMJ
Dalling, JW
AF Lasso, Eloisa
Engelbrecht, Bettina M. J.
Dalling, James W.
TI When sex is not enough: ecological correlates of resprouting capacity in
congeneric tropical forest shrubs
SO OECOLOGIA
LA English
DT Article
DE Asexual reproduction; Life history; Piper; Seed germination; Shade
tolerance
ID RAIN-FOREST; SEED-GERMINATION; LIFE-HISTORY; PLANT-COMMUNITIES; BREEDING
SYSTEMS; TREE DIVERSITY; STARCH STORAGE; CLONAL GROWTH; ROOT STARCH;
TRADE-OFFS
AB In moist tropical forests resprouting may be an important component of life history, contributing to asexual reproduction through the clonal spread of individuals derived from shoot fragments. However, in contrast to other ecosystems where resprouting is common, the ecological correlates of resprouting capacity in tropical forests remain largely unexplored. In this study we characterized shade tolerance, resprouting capacity and sexual reproductive success of eight co-occurring Piper species from lowland forests of Panama. In field experiments we found that shade-tolerant Piper species had a higher capacity to regenerate from excised or pinned stem fragments than light-demanding species in both gap and understory light conditions. In contrast, shade-tolerant species had lower recruitment probabilities from seeds, as a consequence of lower initial seed viability, and lower seedling emergence rates. All Piper species needed gap conditions for successful seedling establishment. Of 8,000 seeds sown in the understory only 0.2% emerged. In gaps, seed germination of light-demanding species was between 10 and 50%, whereas for shade-tolerant species it was 0.5-9.8%. We propose that the capacity to reproduce asexually from resprouts could be adaptive for shade-tolerant species that are constantly exposed to damage from falling litter in the understory. Resprouting may allow Piper populations to persist and spread despite the high rate of pre-dispersal seed predation and low seed emergence rates. Across Piper species, we detected a trade-off between resprouting capacity and the annual viable seed production per plant but not with annual seed mass produced per plant. This suggests that species differences in sexual reproductive success may not necessarily result from differential resource allocation. Instead we suggest that low sexual reproductive success in the understory may in part reflect reduced genetic diversity in populations undergoing clonal growth, resulting in self-fertilization and in-breeding depression.
C1 [Lasso, Eloisa; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
[Lasso, Eloisa; Engelbrecht, Bettina M. J.; Dalling, James W.] Smithsonian Trop Res Inst, Ancon, Panama.
[Engelbrecht, Bettina M. J.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA.
RP Lasso, E (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
EM elasso@illinois.edu
RI Engelbrecht, Bettina/E-9914-2012;
OI Lasso, Eloisa/0000-0003-4586-8674
FU Smithsonian Tropical Research Institute; SENACYT-IFARHU; University of
Illinois at Urbana-Champaign
FX We thank J. Wright, and C. Augspurger for their advice, suggestions and
early comments in this manuscript, and A. Morris, E. Sanchez, B. Wolf,
D. Kikuchi and J. Sousa for help with fieldwork. Financial support for
this work came from a Smithsonian Tropical Research Institute short-term
and a pre-doctoral fellowship, a SENACYT-IFARHU doctoral fellowship and
from the University of Illinois at Urbana-Champaign. The experiments
comply with the current laws of Panama.
NR 77
TC 14
Z9 15
U1 2
U2 19
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
EI 1432-1939
J9 OECOLOGIA
JI Oecologia
PD AUG
PY 2009
VL 161
IS 1
BP 43
EP 56
DI 10.1007/s00442-009-1353-6
PG 14
WC Ecology
SC Environmental Sciences & Ecology
GA 462IT
UT WOS:000267345500005
PM 19412623
ER
PT J
AU Dalling, JW
Pearson, TRH
Ballesteros, J
Sanchez, E
Burslem, DFRP
AF Dalling, James W.
Pearson, T. R. H.
Ballesteros, J.
Sanchez, E.
Burslem, D. F. R. P.
TI Habitat partitioning among neotropical pioneers: a consequence of
differential susceptibility to browsing herbivores?
SO OECOLOGIA
LA English
DT Article
DE Herbivory; Growth; Cecropia; Browsing; Ant-plant
ID TROPICAL FOREST; NEUTRAL THEORY; TREE; CECROPIA; GROWTH; DEFENSE;
DIVERSITY; ABUNDANCE; AZTECA; ESTABLISHMENT
AB Four species of fast-growing pioneer tree species in the genus Cecropia exist in the forests in central Panama. Cecropia insignis is dominant in old-growth forests but absent from nearby secondary forests; C. obtusifolia, and C. peltata are abundant in secondary forests but rare in old-growth forest, and C. longipes is uncommon in both. To determine whether Cecropia habitat associations are a consequence of local dispersal or differences in recruitment success, we grew seedlings of these species in common gardens in large treefall gaps in secondary and old-growth forest. In contrast to the observed adult distribution, only C. insignis grew significantly over 16 months in secondary forests; remaining species were heavily browsed by herbivores. C. insignis also grew and survived best in old-growth forest. Differences in susceptibility to herbivory did not result from an ant defence mutualism; none of the plants were colonised by ants during the experiment. To test whether C. insignis, the species least susceptible to herbivory, trades off investment in growth in favour of defence, we also grew the four Cecropia species in a screened growing house under light conditions comparable to large forest gaps. Contrary to expectation, species growth rates were similar; only C. peltata grew significantly faster than C. insignis. These results suggest that (1) conditions in similar to 40-year-old secondary forests no longer support the recruitment of Cecropia species, which are canopy dominants there; and (2) among congeners, differences in plant traits with little apparent cost to growth can have large impacts on recruitment by affecting palatability to herbivores.
C1 [Dalling, James W.] Univ Illinois Champaign Urbana, Dept Plant Biol, Urbana, IL 61801 USA.
[Dalling, James W.; Ballesteros, J.; Sanchez, E.] Smithsonian Trop Res Inst, Balboa 084303092, Panama.
[Pearson, T. R. H.; Burslem, D. F. R. P.] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland.
RP Dalling, JW (reprint author), Univ Illinois Champaign Urbana, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA.
EM dallingj@life.uiuc.edu
OI Burslem, David/0000-0001-6033-0990
FU University of Illinois; Leverhulme Trust; Natural Environment Research
Council; National Science Foundation [DEB 0343953]; Smithsonian Tropical
Research Institute
FX We thank the University of Illinois, the Leverhulme Trust, the Natural
Environment Research Council, the National Science Foundation (DEB
0343953) and the Smithsonian Tropical Research Institute for financial
support, and N. Brokaw and two anonymous reviewers for comments on an
earlier version of this manuscript. Experiments conducted here comply
with the laws of the Government of Panama.
NR 48
TC 3
Z9 3
U1 0
U2 14
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD AUG
PY 2009
VL 161
IS 2
BP 361
EP 370
DI 10.1007/s00442-009-1385-y
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 477VW
UT WOS:000268548000014
PM 19504125
ER
PT J
AU Farnsworth, NR
Cassileth, B
Weaver, C
Birt, DF
Rosenthal, J
Raskin, I
Barrows, L
Capson, T
Cao, SG
AF Farnsworth, Norman R.
Cassileth, Barrie
Weaver, Connie
Birt, Diane F.
Rosenthal, Joshua
Raskin, Ilya
Barrows, Louis
Capson, Todd
Cao, Shugeng
TI Symposium proceedings for the 48(th) Annual Meeting, Society for
Economic Botany Lake Forest College, Chicago - June 4, 2007 Introduction
SO PHARMACEUTICAL BIOLOGY
LA English
DT Editorial Material
C1 [Farnsworth, Norman R.] Univ Illinois, Coll Pharm, NIH, Ctr Bot Dietary Supplements Res Womens Hlth, Chicago, IL 60612 USA.
[Cassileth, Barrie] Mem Sloan Kettering Canc Ctr, Integrat Med Serv, New York, NY 10021 USA.
[Weaver, Connie] Purdue Univ, Dept Foods & Nutr, W Lafayette, IN 47907 USA.
[Birt, Diane F.] Iowa State Univ, Iowa Ctr Res Bot Dietary Supplements, Ames, IA 50011 USA.
[Rosenthal, Joshua] NIH, Div Int Training & Res, Bethesda, MD 20892 USA.
[Rosenthal, Joshua] NIH, ICBG Program, Fogarty Int Ctr, Bethesda, MD 20892 USA.
[Raskin, Ilya] Rutgers State Univ, Cook Coll, New Brunswick, NJ 08901 USA.
[Barrows, Louis] Univ Utah, Coll Pharm, Dept Pharmacol & Toxicol, Salt Lake City, UT 84112 USA.
[Capson, Todd] Smithsonian Trop Res Inst, Panama City, Panama.
[Cao, Shugeng] Virginia Polytech Inst & State Univ, Dept Chem, Blacksburg, VA 24061 USA.
RP Farnsworth, NR (reprint author), Univ Illinois, Coll Pharm, NIH, Ctr Bot Dietary Supplements Res Womens Hlth, 833 S Wood St, Chicago, IL 60612 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1388-0209
J9 PHARM BIOL
JI Pharm. Biol.
PD AUG
PY 2009
VL 47
IS 8
BP 753
EP 753
DI 10.1080/13880200903013583
PG 1
WC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy
SC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy
GA 490EN
UT WOS:000269481300016
ER
PT J
AU Barrows, LR
Matainaho, TK
Ireland, CM
Miller, S
Carter, GT
Bugni, T
Rai, P
Gideon, O
Manoka, B
Piskaut, P
Banka, R
Kiapranis, R
Noro, JN
Pond, CD
Andjelic, CD
Koch, M
Harper, MK
Powan, E
Pole, AR
Jensen, JB
AF Barrows, L. R.
Matainaho, T. K.
Ireland, C. M.
Miller, S.
Carter, G. T.
Bugni, T.
Rai, P.
Gideon, O.
Manoka, B.
Piskaut, P.
Banka, R.
Kiapranis, R.
Noro, J. N.
Pond, C. D.
Andjelic, C. D.
Koch, M.
Harper, M. K.
Powan, E.
Pole, A. R.
Jensen, J. B.
TI Making the most of Papua New Guinea's biodiversity: Establishment of an
integrated set of programs that link botanical survey with
pharmacological assessment in "the land of the unexpected"
SO PHARMACEUTICAL BIOLOGY
LA English
DT Article
CT 48th Annual Meeting of the Society-for-Economic-Botany
CY JUN 04-07, 2007
CL Lake Forest Coll, Chicago, IL
SP Soc Econ Bot
HO Lake Forest Coll
DE International Cooperative Biodiversity Group; botanical survey;
traditional medicine; drug discovery; Papua New Guinea
ID MYCOBACTERIUM-TUBERCULOSIS; SYSTEM; DISCOVERY; ASSAY; IDENTIFICATION;
EXTRACT; VIRUS
AB An integrated and coordinated set of programs has been established to meet International Cooperative Biodiversity Group (ICBG) goals in Papua New Guinea (PNG). Here we give an overview of the PNG ICBG and focus on the key elements and major steps taken to establish a program necessary for the pharmacological assessment of botanicals and traditional medicines in PNG and, by extrapolation, in other developing countries.
C1 [Barrows, L. R.; Pond, C. D.; Andjelic, C. D.; Koch, M.; Pole, A. R.; Jensen, J. B.] Univ Utah, Dept Pharmacol & Toxicol, Salt Lake City, UT 84112 USA.
[Matainaho, T. K.; Rai, P.; Noro, J. N.; Powan, E.] Univ Papua New Guinea, Sch Med & Hlth Sci, NCD, Port Moresby, Papua N Guinea.
[Ireland, C. M.; Bugni, T.; Harper, M. K.] Univ Utah, Dept Med Chem, Salt Lake City, UT 84112 USA.
[Miller, S.] Smithsonian Inst, Washington, DC 20560 USA.
[Carter, G. T.] Wyeth Res Labs, Pearl River, NY USA.
[Gideon, O.; Manoka, B.; Piskaut, P.] Univ Papua New Guinea, NCD, Sch Nat & Phys Sci, Port Moresby, Papua N Guinea.
[Banka, R.; Kiapranis, R.] Papua New Guinea Forest Res Inst, Lae, Papua N Guinea.
RP Barrows, LR (reprint author), Univ Utah, Dept Pharmacol & Toxicol, 300 S 2000 E, Salt Lake City, UT 84112 USA.
EM lbarrows@pharm.utah.edu
OI Miller, Scott/0000-0002-4138-1378
FU FIC NIH HHS [U01 TW006671, U01 TW006671-05]; NCRR NIH HHS [S10
RR014768-01]
NR 44
TC 6
Z9 6
U1 0
U2 4
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1388-0209
J9 PHARM BIOL
JI Pharm. Biol.
PD AUG
PY 2009
VL 47
IS 8
BP 795
EP 808
DI 10.1080/13880200902991599
PG 14
WC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy
SC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy
GA 490EN
UT WOS:000269481300024
PM 20016761
ER
PT J
AU Hohensee, MA
Lehnert, R
Phillips, DF
Walsworth, RL
AF Hohensee, Michael A.
Lehnert, Ralf
Phillips, David F.
Walsworth, Ronald L.
TI Limits on isotropic Lorentz violation in QED from collider physics
SO PHYSICAL REVIEW D
LA English
DT Review
ID STANDARD-MODEL EXTENSION; CPT VIOLATION; P(P)OVER-BAR COLLISIONS;
E(+)E(-) COLLISIONS; ROOT-S=1.96 TEV; ISOLATED PHOTON; CROSS-SECTION;
TESTS; ELECTRODYNAMICS; INVARIANCE
AB We consider the possibility that Lorentz violation can generate differences between the limiting velocities of light and charged matter. Such effects would lead to efficient vacuum Cherenkov radiation or rapid photon decay. The absence of such effects for 104.5 GeV electrons at the Large Electron Positron collider and for 300 GeV photons at the Tevatron therefore constrains this type of Lorentz breakdown. Within the context of the standard-model extension, these ideas imply an experimental bound at the level of -5.8 x 10(-12) <= (kappa) over tilde (tr) - (4/3)c(e)(00) <= 1.2 x 10(-11) tightening existing laboratory measurements by 3-4 orders of magnitude. Prospects for further improvements with terrestrial and astrophysical methods are discussed.
C1 [Hohensee, Michael A.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Lehnert, Ralf] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Lehnert, Ralf] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hohensee, MA (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
OI Hohensee, Michael/0000-0002-8106-4502
FU European Commission [MOIFCT2005-008687]; CONACyT [55310]; National
Science Foundation
FX R. L. is grateful to B. Altschul, F. R. Klinkhamer, and M. Schreck for
helpful discussions. This work is supported in part by the European
Commission under Grant No. MOIFCT2005-008687, by CONACyT under Grant No.
55310, and by the National Science Foundation.
NR 149
TC 55
Z9 55
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD AUG
PY 2009
VL 80
IS 3
AR 036010
DI 10.1103/PhysRevD.80.036010
PG 11
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 492FU
UT WOS:000269641100102
ER
PT J
AU Slatyer, TR
Padmanabhan, N
Finkbeiner, DP
AF Slatyer, Tracy R.
Padmanabhan, Nikhil
Finkbeiner, Douglas P.
TI CMB constraints on WIMP annihilation: Energy absorption during the
recombination epoch
SO PHYSICAL REVIEW D
LA English
DT Article
ID RAY POSITRON FRACTION; DARK-MATTER; COSMIC-RAYS; COSMOLOGICAL DISTANCES;
PAIR PRODUCTION; CROSS-SECTIONS; GAMMA-RAYS; ELECTRONS; IMPACT;
BREMSSTRAHLUNG
AB We compute in detail the rate at which energy injected by dark matter (DM) annihilation heats and ionizes the photon-baryon plasma at z similar to 1000, and provide accurate fitting functions over the relevant redshift range for a broad array of annihilation channels and DM masses. The resulting perturbations to the ionization history can be constrained by measurements of the CMB temperature and polarization angular power spectra. We show that models which fit recently measured excesses in 10-1000 GeV electron and positron cosmic rays are already close to the 95% confidence limits from WMAP. The recently launched Planck satellite will be capable of ruling out a wide range of DM explanations for these excesses. In models of dark matter with Sommerfeld-enhanced annihilation, where <> rises with decreasing WIMP velocity until some saturation point, the WMAP5 constraints imply that the enhancement must be close to saturation in the neighborhood of the Earth.
C1 [Slatyer, Tracy R.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Padmanabhan, Nikhil] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Slatyer, TR (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
EM tslatyer@fas.harvard.edu; NPadmanabhan@lbl.gov;
dfinkbeiner@cfa.harvard.edu
RI Padmanabhan, Nikhil/A-2094-2012
NR 70
TC 221
Z9 221
U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD AUG
PY 2009
VL 80
IS 4
AR 043526
DI 10.1103/PhysRevD.80.043526
PG 16
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 492FX
UT WOS:000269641400041
ER
PT J
AU Marsden, BG
AF Marsden, Brian G.
TI Orbital properties of Jupiter-family comets
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Comets; Jupiter family; Centaurs; Tisserand criterion
ID SHORT-PERIOD COMETS; NONGRAVITATIONAL FORCES; OUTGASSING ASYMMETRY;
MODEL-CALCULATIONS; MOTION; ENCKE; BELT; ACCELERATIONS; PRECESSION;
NUCLEUS
AB The history of "comet families", in particular the Jupiter comet family, is reviewed, together with ways in which the Jupiter family has been defined. New criteria are proposed, particularly with regard to distinguishing Jupiter-family comets (JFCs) from centaurs. The effect of nongravitational forces on JFCs is also discussed. Published by Elsevier Ltd.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Marsden, BG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bmarsden@cfa.harvard.edu
NR 61
TC 2
Z9 2
U1 1
U2 2
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 AUG
PY 2009
VL 57
IS 10
BP 1098
EP 1105
DI 10.1016/j.pss.2008.12.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 484HT
UT WOS:000269035900002
ER
PT J
AU Lonsdale, CJ
Cappallo, RJ
Morales, MF
Briggs, FH
Benkevitch, L
Bowman, JD
Bunton, JD
Burns, S
Corey, BE
Desouza, L
Doeleman, SS
Derome, M
Deshpande, A
Gopala, MR
Greenhill, LJ
Herne, DE
Hewitt, JN
Kamini, PA
Kasper, JC
Kincaid, BB
Kocz, J
Kowald, E
Kratzenberg, E
Kumar, D
Lynch, MJ
Madhavi, S
Matejek, M
Mitchell, DA
Morgan, E
Oberoi, D
Ord, S
Pathikulangara, J
Prabu, T
Rogers, AEE
Roshi, A
Salah, JE
Sault, RJ
Shankar, NU
Srivani, KS
Stevens, J
Tingay, S
Vaccarella, A
Waterson, M
Wayth, RB
Webster, RL
Whitney, AR
Williams, A
Williams, C
AF Lonsdale, Colin J.
Cappallo, Roger J.
Morales, Miguel F.
Briggs, Frank H.
Benkevitch, Leonid
Bowman, Judd D.
Bunton, John D.
Burns, Steven
Corey, Brian E.
deSouza, Ludi
Doeleman, Sheperd S.
Derome, Mark
Deshpande, Avinash
Gopala, Modavanatt Ramakrishna
Greenhill, Lincoln J.
Herne, David Edwin
Hewitt, Jacqueline N.
Kamini, P. A.
Kasper, Justin C.
Kincaid, Barton B.
Kocz, Jonathan
Kowald, Errol
Kratzenberg, Eric
Kumar, Deepak
Lynch, Mervyn J.
Madhavi, S.
Matejek, Michael
Mitchell, Daniel A.
Morgan, Edward
Oberoi, Divya
Ord, Steven
Pathikulangara, Joseph
Prabu, T.
Rogers, Alan E. E.
Roshi, Anish
Salah, Joseph E.
Sault, Robert J.
Shankar, N. Udaya
Srivani, K. S.
Stevens, Jamie
Tingay, Steven
Vaccarella, Annino
Waterson, Mark
Wayth, Randall B.
Webster, Rachel L.
Whitney, Alan R.
Williams, Andrew
Williams, Christopher
TI The Murchison Widefield Array: Design Overview
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Antenna arrays; astronomy; calibration; imaging; ionosphere
ID TELESCOPE; HEALPIX
AB The Murchison Widefield Array is a dipole-based aperture array synthesis telescope designed to operate in the 80-300 MHz frequency range. It is capable of a wide range of science investigations but is initially focused on three key science projects: detection and characterization of three-dimensional brightness temperature fluctuations in the 21 cm line of neutral hydrogen during the epoch of reionization (EoR) at redshifts from six to ten; solar imaging and remote sensing of the inner heliosphere via propagation effects on signals from distant background sources; and high-sensitivity exploration of the variable radio sky. The array design features 8192 dual-polarization broadband active dipoles, arranged into 512 "tiles" comprising 16 dipoles each. The tiles are quasi-randomly distributed over an aperture 1.5 km in diameter, with a small number of outliers extending to 3 km. All tile-tile baselines are correlated in custom field-programmable gate array based hardware, yielding a Nyquist-sampled instantaneous monochromatic uv coverage and unprecedented point spread function quality. The correlated data are calibrated in real time using novel position-dependent self-calibration algorithms. The array is located in the Murchison region of outback Western Australia. This region is characterized by extremely low population density and a superbly radio-quiet environment, allowing full exploitation of the instrumental capabilities.
C1 [Lonsdale, Colin J.; Cappallo, Roger J.; Benkevitch, Leonid; Corey, Brian E.; Doeleman, Sheperd S.; Derome, Mark; Kincaid, Barton B.; Kratzenberg, Eric; Oberoi, Divya; Rogers, Alan E. E.; Salah, Joseph E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA.
[Morales, Miguel F.; Bowman, Judd D.] MIT, Cambridge, MA 02139 USA.
[Briggs, Frank H.; Kocz, Jonathan; Kowald, Errol; Vaccarella, Annino; Waterson, Mark] Australian Natl Univ, Canberra, ACT, Australia.
[Bunton, John D.; deSouza, Ludi; Pathikulangara, Joseph] Commonwealth Sci & Ind Res Org, Epping, NSW, Australia.
[Burns, Steven] Burns Ind Inc, Nashua, NH 03064 USA.
[Deshpande, Avinash; Gopala, Modavanatt Ramakrishna; Kamini, P. A.; Kumar, Deepak; Madhavi, S.; Prabu, T.; Roshi, Anish; Shankar, N. Udaya; Srivani, K. S.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Greenhill, Lincoln J.; Kasper, Justin C.; Mitchell, Daniel A.; Ord, Steven; Wayth, Randall B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Herne, David Edwin; Lynch, Mervyn J.; Tingay, Steven] Curtin Univ Technol, Perth, WA, Australia.
[Hewitt, Jacqueline N.; Matejek, Michael; Morgan, Edward; Williams, Christopher] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Sault, Robert J.; Webster, Rachel L.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Stevens, Jamie] Univ Tasmania, Hobart, Tas 7001, Australia.
[Williams, Andrew] Univ Western Australia, Perth, WA 6009, Australia.
RP Lonsdale, CJ (reprint author), MIT, Haystack Observ, Westford, MA 01886 USA.
EM cjl@haystack.mit.edu
RI Bunton, John/A-4944-2008; Tingay, Steven/B-5271-2013; Waterson,
Mark/B-7352-2013; Ord, Stephen/C-6138-2013; Kasper, Justin/D-1152-2010;
Williams, Andrew/K-2931-2013; Deshpande, Avinash/D-4868-2012;
Udayashankar , N/D-4901-2012; Astronomy & Astrophysics Group, Raman Res
Institute/D-4046-2012; Wayth, Randall/B-2444-2013
OI Waterson, Mark/0000-0002-0192-2686; Kasper, Justin/0000-0002-7077-930X;
Williams, Andrew/0000-0001-9080-0105; Kocz,
Jonathon/0000-0003-0249-7586; Wayth, Randall/0000-0002-6995-4131
FU National Science Foundation [AST-0457585]; Australian Research Council
[LE775621, LE882938, DP345001]; U.S. Air Force Office of Scientific
Research [FA9550-0510247]
FX This work was supported by the National Science Foundation under Grant
AST-0457585; the Australian Research Council under Grants LE775621,
LE882938, and DP345001; and the U.S. Air Force Office of Scientific
Research under Grant FA9550-0510247.
NR 13
TC 162
Z9 162
U1 0
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0018-9219
J9 P IEEE
JI Proc. IEEE
PD AUG
PY 2009
VL 97
IS 8
BP 1497
EP 1506
DI 10.1109/JPROC.2009.2017564
PG 10
WC Engineering, Electrical & Electronic
SC Engineering
GA 472WW
UT WOS:000268164600015
ER
PT J
AU Wayth, RB
Greenhill, LJ
Briggs, FH
AF Wayth, Randall B.
Greenhill, Lincoln J.
Briggs, Frank H.
TI A GPU-based Real-time Software Correlation System for the Murchison
Widefield Array Prototype
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
AB Modern graphics processing units (GPUs) are inexpensive commodity hardware that offer Tflop/s theoretical computing capacity. GPUs are well suited to many compute-intensive tasks including digital signal processing. We describe the implementation and performance of a GPU-based digital correlator for radio astronomy. The correlator is implemented using the NVIDIA CUDA development environment. We evaluate three design options on two generations of NVIDIA hardware. The different designs utilize the internal registers, shared memory, and multiprocessors in different ways. We find that optimal performance is achieved with the design that minimizes global memory reads on recent generations of hardware. The GPU-based correlator outperforms a single-threaded CPU equivalent by a factor of 60 for a 32-antenna array, and runs on commodity PC hardware. The extra compute capability provided by the GPU maximizes the correlation capability of a PC while retaining the fast development time associated with using standard hardware, networking, and programming languages. In this way, a GPU-based correlation system represents a middle ground in design space between high performance, custom-built hardware, and pure CPU-based software correlation. The correlator was deployed at the Murchison Widefield Array 32-antenna prototype system where it ran in real time for extended periods. We briefly describe the data capture, streaming, and correlation system for the prototype array.
C1 [Wayth, Randall B.; Greenhill, Lincoln J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Briggs, Frank H.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
RP Wayth, RB (reprint author), Curtin Inst Radio Astron, GPO Box U1987, Perth, WA 6845, Australia.
EM rwayth@cfa.harvard.edu
RI Wayth, Randall/B-2444-2013
OI Wayth, Randall/0000-0002-6995-4131
FU National Science Foundation [AST-0457585, PHY-0835713]
FX This work was in part supported by grants AST-0457585 and PHY-0835713 of
the National Science Foundation.
NR 8
TC 22
Z9 24
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2009
VL 121
IS 882
BP 857
EP 865
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 480XH
UT WOS:000268770100005
ER
PT J
AU Robeck, TR
Steinman, KJ
Greenwell, M
Ramirez, K
Van Bonn, W
Yoshioka, M
Katsumata, E
Dalton, L
Osborn, S
O'Brien, JK
AF Robeck, T. R.
Steinman, K. J.
Greenwell, M.
Ramirez, K.
Van Bonn, W.
Yoshioka, M.
Katsumata, E.
Dalton, L.
Osborn, S.
O'Brien, J. K.
TI Seasonality, estrous cycle characterization, estrus synchronization,
semen cryopreservation, and artificial insemination in the Pacific
white-sided dolphin (Lagenorhynchus obliquidens)
SO REPRODUCTION
LA English
DT Article
ID BOTTLE-NOSED-DOLPHIN; BELUGA DELPHINAPTERUS-LEUCAS;
TURSIOPS-TRUNCATUS-ADUNCAS; WHALES ORCINUS-ORCA; REPRODUCTIVE
TECHNOLOGY; ENZYME-IMMUNOASSAY; ALLYL TRENBOLONE; RESOURCE BANKS;
SPERMATOZOA; HORMONE
AB The reproductive physiology of the Pacific white-sided dolphin, Lagenorhynchus obliquidens, was characterized to facilitate the development of artificial insemination (Al) using cryopreserved spermatozoa. Specific objectives were to: 1) describe reproductive seasonality of the Pacific white sided dolphins; 2) describe urinary LH and ovarian steroid metabolites during the estrous cycle; 3) correlate LH and ovarian steroidal metabolite patterns to ultrasound-monitored follicular growth and ovulation; and 4) assess the efficacy of synchronizing estrus, sperm collection/cryopreservation, and intrauterine insemination. Ovulations (64%, n=37) and conceptions (83%, n=18) occurred from August to October. Peak mean serum testosterone (24 ng/ml), cross-sectional testicular area (41.6 cm(2)), and sperm concentration (144.3 x 10(7) sperm/ml) occurred in July, August, and September respectively. Spermatozoa were only found in ejaculates from July to October. Estrous cycles (n=22) were 31 d long and were comprised of a 10 d follicular and 21 d luteal phase. Ovulation occurred 31.2 h after the onset of the LH surge and 19.3 h after the LH peak. Follicular diameter and circumference within 12 h of ovulation were 1.52 and 4.66 cm respectively. Estrus synchronization attempts with altrenogest resulted in 17 (22%) ovulatory cycles with ovulation occurring 21 d post-altrenogest. Ten Al attempts using cryopreserved semen resulted in five pregnancies (50%). The mean gestation length was 356 days (range 348-367). These data provide new information on the Pacific white-sided dolphin's reproductive physiology and collectively enabled the first application of Al in this species. Reproduction (2009) 138 391-405
C1 [Robeck, T. R.; Steinman, K. J.; O'Brien, J. K.] Busch Entertainment Corp, SeaWorld & Busch Gardens Reprod Res Ctr, San Diego, CA 92109 USA.
[Steinman, K. J.] Natl Zool Pk, Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA.
[Greenwell, M.; Ramirez, K.; Van Bonn, W.] John G Shedd Aquarium, Chicago, IL 60605 USA.
[Yoshioka, M.] Mie Univ, Lab Fish Culture, Grad Sch Bioresources, Tsu, Mie 5148507, Japan.
[Katsumata, E.] Kamogawa SeaWorld, Chiba 2960041, Japan.
[Dalton, L.; Osborn, S.] SeaWorld San Antonio, San Antonio, TX 78259 USA.
[O'Brien, J. K.] Univ Sydney, Fac Vet Sci, Ctr Adv Technol Anim Genet & Reprod, Sydney, NSW 2006, Australia.
RP Robeck, TR (reprint author), Busch Entertainment Corp, SeaWorld & Busch Gardens Reprod Res Ctr, San Diego, CA 92109 USA.
EM todd.robeck@seaworld.com
FU SeaWorld Corp.; John G Shedd Aquarium
FX This project was supported by SeaWorld Corp. and John G Shedd Aquarium.
NR 48
TC 23
Z9 25
U1 4
U2 22
PU BIO SCIENTIFICA LTD
PI BRISTOL
PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT,
ENGLAND
SN 1470-1626
J9 REPRODUCTION
JI Reproduction
PD AUG
PY 2009
VL 138
IS 2
BP 391
EP 405
DI 10.1530/REP-08-0528
PG 15
WC Developmental Biology; Reproductive Biology
SC Developmental Biology; Reproductive Biology
GA 475FT
UT WOS:000268344700020
PM 19494046
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI FROM THE CASTLE Ways We Serve
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD AUG
PY 2009
VL 40
IS 5
BP 22
EP 22
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 477LE
UT WOS:000268519800011
ER
PT J
AU Torres-Carvajal, O
AF Torres-Carvajal, Omar
TI Non-parametric bootstrapping of partitioned datasets
SO TAXON
LA English
DT Article
DE non-parametric bootstrapping; partitioned datasets
ID LIKELIHOOD ANALYSIS; PHYLOGENY; CONFIDENCE; LIZARDS; MODELS
AB Non-parametric bootstrapping is one of the most commonly used methods for branch support assessment. Unlike Bayesian posterior probability values, which are influenced by apriori data partitioning, non-parametric bootstrapping is usually applied to Unpartitioned (combined) datasets. The resulting bootstrap support values are misleading in that they do not measure how well clades are Supported by all the partitions, unless all partitions are equal in size (i.e., number of characters). Since most empirical studies include data partitions that are heterogeneous ill Size, Our Current bootstrapping approach for partitioned datasets (i.e., bootstrapping the combined dataset) is not adequate. Here I propose a simple modification to non-parametric bootstrapping that takes a priori data partitioning into account by obtaining bootstrap replicates for each partition separately and combining them in Such a way that the size (i.e., number of characters) of each partition is taken into account. With this "corrected" bootstrap support value, characters from smaller partitions will have greater influence on final bootstrap values, and those in larger partitions relatively less influence than they would for unpartitioned data.
C1 [Torres-Carvajal, Omar] Pontificia Univ Catolica Ecuador, Escuela Biol, Quito, Ecuador.
[Torres-Carvajal, Omar] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Torres-Carvajal, O (reprint author), Pontificia Univ Catolica Ecuador, Escuela Biol, Ave 12 Octubre & Roca,Apartado 17-01-2184, Quito, Ecuador.
EM omartorcar@gmail.com
NR 16
TC 0
Z9 0
U1 0
U2 5
PU INT ASSOC PLANT TAXONOMY
PI VIENNA
PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA
SN 0040-0262
J9 TAXON
JI Taxon
PD AUG
PY 2009
VL 58
IS 3
BP 955
EP 958
PG 4
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 493YH
UT WOS:000269774900022
ER
PT J
AU Dorr, LJ
Pilz, GE
Boggan, J
AF Dorr, Laurence J.
Pilz, George E.
Boggan, John
TI The transfer of types from the Escuela Agricola Panamericana to the US
National Herbarium in 1956 by Louis O. Williams
SO TAXON
LA English
DT Editorial Material
DE Central American plants; Escuela Agricola Panamericana; Louis O.
Williams; US National Herbarium
AB In 1956, Louis O. Williams transferred type specimens of Central American and Mexican plants that had been deposited in the Escuela Agricola Panamericana (EAP), Honduras to the U.S. National Herbarium (US), Smithsonian Institution, Washington, D.C., U.S.A. With only a few exceptions, the specimens typified names of taxa that had been described by Williams and his colleagues in Honduras, who had stated in their publications (numerous articles in the scientific serial Ceiba and the book The Rain Forests of Golfo Dulce) that the "types" (i.e., holotypes) were deposited in EAR This transfer, which was neither publicly announced nor otherwise previously well-documented, has led to confusion regarding the present location of the holotypes of many names. Details regarding Williams's transaction and an accounting of the 195 collections and 219 specimens involved are presented.
C1 [Dorr, Laurence J.; Boggan, John] Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, Washington, DC 20013 USA.
[Pilz, George E.] Escuela Agr Panamer, Tegucigalpa, Honduras.
RP Dorr, LJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, POB 37012, Washington, DC 20013 USA.
EM dorrl@si.edu
NR 25
TC 1
Z9 1
U1 0
U2 3
PU INT ASSOC PLANT TAXONOMY-IAPT
PI BRATISLAVA
PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23
BRATISLAVA, SLOVAKIA
SN 0040-0262
EI 1996-8175
J9 TAXON
JI Taxon
PD AUG
PY 2009
VL 58
IS 3
BP 993
EP 1001
PG 9
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 493YH
UT WOS:000269774900030
ER
PT J
AU Diaz-Marrero, AR
Porras, G
Cueto, M
D'Croz, L
Lorenzo, M
San-Martin, A
Darias, J
AF Diaz-Marrero, Ana R.
Porras, Gina
Cueto, Mercedes
D'Croz, Luis
Lorenzo, Manuel
San-Martin, Aurelio
Darias, J.
TI Leptogorgolide, a biogenetically interesting 1,4-diketo-cembranoid that
reinforces the oxidation profile of C-18 as taxonomical marker for
octocorals
SO TETRAHEDRON
LA English
DT Article
DE Leptogorgia; Leptogorgolide; 1,4-Diketo-cembranoid
ID NATURAL-PRODUCTS; CONFIGURATION; ASSIGNMENT; DITERPENES; CHEMISTRY; NMR
AB The cembranoid 1 and the furanocembranolides 2-4 along with the known pukalide were isolated from Leptogorgia sp. and their structures determined spectroscopically. The 1,4-diketo-cembranoid 1 follows an oxidation pattern of C-18 that reinforces the concept of oxidation profile of C-18 as taxonomical marker for octocorals. The co-occurrence within a species of furanocembranolide/1,4-diketo-cembranoid congeners 1/2-4 raises the question about which one is the biogenetic precursor. A biogenetic pathway is proposed. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Diaz-Marrero, Ana R.; Porras, Gina; Cueto, Mercedes; Darias, J.] CSIC, Inst Prod Nat & Agrobiol, Tenerife 38206, Spain.
[D'Croz, Luis] Smithsonian Trop Res Inst, Balboa, Panama.
[D'Croz, Luis] Univ Panama, Estafeta Univ, Dept Biol Marina & Limnol, Panama City, Panama.
[Lorenzo, Manuel] Univ Magallanes, Punta Arenas, Chile.
[San-Martin, Aurelio] Univ Chile, Dept Quim, Santiago, Chile.
RP Diaz-Marrero, AR (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez 3, Tenerife 38206, Spain.
EM ardiaz@ipna.csic.es
RI Diaz-Marrero, Ana/L-2899-2014; Cueto, MERCEDES/L-3185-2014
OI Diaz-Marrero, Ana/0000-0002-8886-7519; Cueto,
MERCEDES/0000-0002-9112-6877
FU Ministerio de Educacion y Ciencia [BIO2007-61745, SAF2006-03004]; DGUI
Gobierno de Canarias [PIO42005, PUB2005/030]; Convenio de Cooperacion
Universidad de Chile-CSIC [2006CL0041]; Programa Juan de la Cierva
(Ministerio de Educacion y Ciencia of Spain)
FX This work was supported by the Ministerio de Educacion y Ciencia
(BIO2007-61745, SAF2006-03004), DGUI Gobierno de Canarias (PIO42005,
PUB2005/030), and Convenio de Cooperacion Universidad de Chile-CSIC,
ref: 2006CL0041. A.R.D.-M. acknowledges financial support from Programa
Juan de la Cierva (Ministerio de Educacion y Ciencia of Spain). The STRI
provided facilities and J. del Rosario provided technical support. The
Government of Panama granted permission for the collection of samples.
NR 16
TC 10
Z9 10
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0040-4020
J9 TETRAHEDRON
JI Tetrahedron
PD AUG 1
PY 2009
VL 65
IS 31
BP 6029
EP 6033
DI 10.1016/j.tet.2009.05.068
PG 5
WC Chemistry, Organic
SC Chemistry
GA 473OL
UT WOS:000268217000022
ER
PT J
AU Zachos, LG
AF Zachos, Louis G.
TI THE SAND DOLLAR PERIARCHUS LYELLI (ECHINOIDEA: CLYPEASTEROIDA:
SCUTELLIFORMES) IN THE CADDELL FORMATION (UPPER EOCENE) OF TEXAS
SO TEXAS JOURNAL OF SCIENCE
LA English
DT Article
AB The occurrence of the sand dollar echinoid Periarchus lyelli in the Upper Eocene Caddell Formation of Texas is confirmed. This extends the geographic range of this Gulf Coast index fossil west from Mississippi to Texas.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA.
RP Zachos, LG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, POB 37012, Washington, DC 20013 USA.
EM lg_zachos@alumni.utexas.net
FU Geology Foundation of the Jackson School of Geosciences at the
University of Texas at Austin; Smithsonian Institution
FX Appreciation is extended to A. Molineux, Texas Natural Science Center,
Austin for assistance with the collections of the Non-Vertebrate
Paleontology Laboratory, and to C. Ciampaglio and T. Yancey for their
critical review of the manuscript. This work was supported by the
Geology Foundation of the Jackson School of Geosciences at the
University of Texas at Austin., and by the Smithsonian Institution
Fellowship Program.
NR 13
TC 0
Z9 0
U1 0
U2 0
PU TEXAS ACAD SCI
PI KERRVILLE
PA CMB 6252, SCHREINER UNIV, KERRVILLE, TX 78028-5697 USA
SN 0040-4403
J9 TEX J SCI
JI Tex. J. Sci.
PD AUG
PY 2009
VL 61
IS 3
BP 181
EP 186
PG 6
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA 637YG
UT WOS:000280854000002
ER
PT J
AU McLaughlin, PA
Lemaitre, R
AF McLaughlin, Patsy A.
Lemaitre, Rafael
TI A NEW CLASSIFICATION FOR THE PYLOCHELIDAE (DECAPODA: ANOMURA:
PAGUROIDEA) AND DESCRIPTIONS OF NEW TAXA
SO RAFFLES BULLETIN OF ZOOLOGY
LA English
DT Article
DE Decapoda; Anomura; Paguroidea; Pylochelidae; new classification;
Pylochelinae; Pomatochelinae Trizochelinae; tribes; new genus; new
species
ID SOUTHEASTERN NEW-ZEALAND; HERMIT-CRABS; CRUSTACEA; PHYLOGENY
AB A new classification is presented based on the results of the recently completed cladistic analysis of the Pylochelidae. The subfamilies Pylochelinae and Pomatochelinae are retained, the latter with the genera Pylocheles and Cheiroplatea; however, the subgenera Xylocheles and Bathycheles are elevated to generic rank together with the nominal subgenus Pylocheles. In addition, one new species, B. phenax, is described in Bathycheles and B. profundus is shown to be conspecific with B. integer. The subfamilies Parapylochelinae, Cancellochelinae, Trizochelinae, and Mixtopagurinae are reduced to ranks of tribes and included in the subfamily Trizochelinae. A new genus Forestocheles is proposed in the tribe Trizochelini. Within the genus Trizocheles, subspecific rank for T. spinosus bathamae is deemed unjustified and this taxon is placed in synonymy with the nominal subspecies T spinosus spinosus. The correct identity of Trizocheles balssi is established and the species mistakenly thought to represent that taxon is described as T. hoensonae, new species. Trizocheles gracilis is found to be conspecific with T. boasi and an additional new species, T. mendanai, is added to the genus. The superfamilial ranks of Cheiroplateoidea, Pomatocheloidea, Pylocheloidea, and Cancellocheloidea proposed by Watabe (2007) are rejected, as is Birgusoidea.
C1 [McLaughlin, Patsy A.] Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA.
[Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP McLaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, 1900 Shannon Point Rd, Anacortes, WA 98221 USA.
EM hermit@fidalgo.net; lemaitrr@si.edu
NR 90
TC 16
Z9 22
U1 0
U2 3
PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES
PI SINGAPORE
PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE
SN 0217-2445
J9 RAFFLES B ZOOL
JI Raffles Bull. Zool.
PD JUL 31
PY 2009
SU 20
BP 159
EP 231
PG 73
WC Zoology
SC Zoology
GA 530GR
UT WOS:000272577700009
ER
PT J
AU Kelley, KA
Cottrell, E
AF Kelley, Katherine A.
Cottrell, Elizabeth
TI Water and the Oxidation State of Subduction Zone Magmas
SO SCIENCE
LA English
DT Article
ID OXYGEN FUGACITIES; REDOX STATES; MANTLE; MELT; FLUIDS; CONSTRAINTS;
WASHINGTON; INCLUSIONS; PERIDOTITE; VOLATILES
AB Mantle oxygen fugacity exerts a primary control on mass exchange between Earth's surface and interior at subduction zones, but the major factors controlling mantle oxygen fugacity (such as volatiles and phase assemblages) and how tectonic cycles drive its secular evolution are still debated. We present integrated measurements of redox-sensitive ratios of oxidized iron to total iron (Fe3+/SFe), determined with Fe K-edge micro-x-ray absorption near-edge structure spectroscopy, and pre-eruptive magmatic H2O contents of a global sampling of primitive undegassed basaltic glasses and melt inclusions covering a range of plate tectonic settings. Magmatic Fe3+/SFe ratios increase toward subduction zones (at ridges, 0.13 to 0.17; at back arcs, 0.15 to 0.19; and at arcs, 0.18 to 0.32) and correlate linearly with H2O content and element tracers of slab-derived fluids. These observations indicate a direct link between mass transfer from the subducted plate and oxidation of the mantle wedge.
C1 [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Kelley, KA (reprint author), Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
EM kelley@gso.uri.edu
RI Kelley, Katherine/J-3728-2013
OI Kelley, Katherine/0000-0002-7516-2683
FU Smithsonian; NSF [EAR-0841108, EAR-0841006, OCE-0644625]; U.S.
Department of Energy Geosciences Division [DE-FG02-92ER14244];
University of Chicago Consortium for Advanced Radiation Sources; DOE
[DE-AC02-98CH10886]
FX This work was supported by a Smithsonian Scholarly Studies Grant to
E.C., a NSF ADVANCE fellowship to K.K., and NSF awards EAR-0841108
(K.K.) and EAR-0841006 (E.C.). NSF award OCE-0644625 provided curatorial
support for marine geological samples at the University of Rhode Island.
Beamline X26A is supported by the U.S. Department of Energy (DOE)
Geosciences Division (grant DE-FG02-92ER14244 to the University of
Chicago, Consortium for Advanced Radiation Sources). Use of the National
Synchrotron Light Source was supported by DOE under contract
no.DE-AC02-98CH10886.
NR 28
TC 208
Z9 213
U1 7
U2 96
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 JUL 31
PY 2009
VL 325
IS 5940
BP 605
EP 607
DI 10.1126/science.1174156
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 477BY
UT WOS:000268493000048
PM 19644118
ER
PT J
AU D'Onghia, E
Besla, G
Cox, TJ
Hernquist, L
AF D'Onghia, Elena
Besla, Gurtina
Cox, Thomas J.
Hernquist, Lars
TI Resonant stripping as the origin of dwarf spheroidal galaxies
SO NATURE
LA English
DT Article
ID DARK-MATTER; GALACTIC SATELLITES; MILKY-WAY; LOCAL GROUP; CLUSTERS;
EVOLUTION; GAS
AB Dwarf spheroidal galaxies are the most dark-matter-dominated systems in the nearby Universe(1-3) and their origin is one of the outstanding puzzles of how galaxies form. Dwarf spheroidals are poor in gas and stars, making them unusually faint(4-6), and those known as ultra-faint dwarfs(7,8) have by far the lowest measured stellar content of any galaxy(9,10). Previous theories(11) require that dwarf spheroidals orbit near giant galaxies like the Milky Way, but some dwarfs have been observed in the outskirts of the Local Group(12). Here we report simulations of encounters between dwarf disk galaxies and somewhat larger objects. We find that the encounters excite a process, which we term 'resonant stripping', that transforms them into dwarf spheroidals. This effect is distinct from other mechanisms proposed to form dwarf spheroidals, including mergers(13), galaxy galaxy harassment(14), or tidal and ram pressure stripping, because it is driven by gravitational resonances. It may account for some of the observed properties of dwarf spheroidals in the Local Group. Within this framework, dwarf spheroidals should form and interact in pairs, leaving detectable long stellar streams and tails.
C1 [D'Onghia, Elena] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[D'Onghia, Elena; Besla, Gurtina; Cox, Thomas J.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP D'Onghia, E (reprint author), Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
EM edonghia@cfa.harvard.edu
FU EU [MEIF-041569]; NSERC
FX This research was partly supported by an EU Marie Curie Intra-European
Fellowship under contract MEIF-041569 and by an NSERC postgraduate
fellowship. Numerical simulations were performed on the Odyssey
supercomputer at Harvard University.
NR 30
TC 65
Z9 65
U1 0
U2 1
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 30
PY 2009
VL 460
IS 7255
BP 605
EP 607
DI 10.1038/nature08215
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 476PK
UT WOS:000268454300044
ER
PT J
AU Head, JJ
Bloch, JI
Hastings, AK
Bourque, JR
Cadena, EA
Herrera, FA
Polly, PD
Jaramillo, CA
AF Head, Jason J.
Bloch, Jonathan I.
Hastings, Alexander K.
Bourque, Jason R.
Cadena, Edwin A.
Herrera, Fabiany A.
Polly, P. David
Jaramillo, Carlos A.
TI Untitled Reply
SO NATURE
LA English
DT Letter
ID TERRESTRIAL POIKILOTHERMS; TEMPERATURE; MEGALANIA; GIGANTISM
C1 [Head, Jason J.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada.
[Bloch, Jonathan I.; Hastings, Alexander K.; Bourque, Jason R.; Cadena, Edwin A.; Herrera, Fabiany A.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Cadena, Edwin A.; Herrera, Fabiany A.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama.
[Polly, P. David] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
RP Head, JJ (reprint author), Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada.
EM jason.head@utoronto.ca
OI Head, Jason/0000-0002-2237-6901; Polly, P. David/0000-0001-7338-8526
NR 14
TC 2
Z9 3
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 30
PY 2009
VL 460
IS 7255
BP E4
EP E5
DI 10.1038/nature08225
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 476PK
UT WOS:000268454300060
ER
PT J
AU Robinson, H
Skvarla, JJ
AF Robinson, Harold
Skvarla, John J.
TI Studies on the Paleotropical Vernonieae (Asteraceae): additions to the
genus Acilepis from southern Asia
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID LEPIDAPLOA COMPLEX VERNONIEAE; INDIAN COMPOSITAE; GYMNANTHEMINAE
VERNONIEAE; RESTORATION
AB Thirty-three species are recognized in the genus Acilepis with new combinations provided for A. attenuata, A. chiangdaoensis, A. divergens, A. doichangensis, A. fysonii, A. gardneri, A. heynei, A. kingii, A. lobbii, A. namnaoensis, A. nayarii, A. nemoralis, A. ngaoensis, A. ornata, A. peguensis, A. peninsularis, A. principis, A. pseudosutepensis, A. setigera, A. sutepensis, A. thwaitesii, A. tonkinensis, and A. virgata. Acilepis; belcheri is described as new. The rhizomiform structure of the pollen muri is discussed and compared with other Vernonieae in Old World Erlangeinae and in New World Lepidaploinae with similar muri.
C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Skvarla, John J.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA.
[Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA.
RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM robinsoh@si.edu; jskvarla@ou.edu
NR 24
TC 8
Z9 10
U1 1
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 131
EP 145
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300001
ER
PT J
AU Robinson, H
Skvarla, JJ
AF Robinson, Harold
Skvarla, John J.
TI A new genus, Khasianthus, from India, Myanmar, and China (Vernonieae:
Asteraceae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID GYMNANTHEMINAE VERNONIEAE; RESTORATION
AB A new Asian genus of Vernonieae, Khasianthus, is named for Vernonia subsessilis DC. It is most closely related to the primarily African genus Baccharoides Moench.
C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Skvarla, John J.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA.
[Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA.
RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM robinsoh@si.edu; jskvarla@ou.edu
NR 10
TC 5
Z9 6
U1 0
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 146
EP 149
PG 4
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300002
ER
PT J
AU Robinson, H
Skvarla, JJ
AF Robinson, Harold
Skvarla, John J.
TI A new genus, Uniyala, from peninsular India and Sri Lanka (Vernonieae:
Asteraceae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID GYMNANTHEMINAE VERNONIEAE; RESTORATION
AB The genus Uniyala, of southern India and Sri Lanka, is described as new for seven shrubby species, previously placed in Vernonia, with 4- or 5-costate achenes and blunt sweeping hairs on the style branches. The new combinations are Uniyala anceps, U. bourdillonii, U. comorinensis, U. multibracteata, U. ramaswamii, U. salvifolia, and U. wightiana.
C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Skvarla, John J.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA.
[Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA.
RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM robinsoh@si.edu; jskvarla@ou.edu
NR 17
TC 8
Z9 9
U1 0
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 150
EP 154
PG 5
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300003
ER
PT J
AU Funk, VA
Robinson, H
AF Funk, Vicki A.
Robinson, Harold
TI Sampera, a new genus of Liabeae (Compositae or Asteraceae) from the
northern Andes
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB The genus Oligactis (Kunth) Cass. is divided into two genera based on the two former subgenera and a new name was necessary for the non-typical subgenus. DNA sequence data have shown that these two groups are not sister taxa and that each is easily defined by morphological characters that include differences in the habit, position of the inflorescence, and the pubescence of the style branches. Sampera, with eight species, is named in honor of Dr. Cristian Samper, Director of the Natural History Museum, Smithsonian Institution.
C1 [Funk, Vicki A.] Smithsonian Inst, US Natl Herbarium, Dept Bot, Natl Museum Nat Hist,MRC 166, Washington, DC 20013 USA.
RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, Dept Bot, Natl Museum Nat Hist,MRC 166, POB 37012, Washington, DC 20013 USA.
EM funkv@si.edu; robinsoh@si.edu
NR 12
TC 5
Z9 5
U1 0
U2 0
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 155
EP 161
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300004
ER
PT J
AU Judkins, H
Ingrao, DA
Roper, CFE
AF Judkins, Heather
Ingrao, Debra A.
Roper, Clyde F. E.
TI First records of Asperoteuthis acanthoderma (Lu, 1977) (Cephalopoda:
Oegopsida: Chiroteuthidae), from the North Atlantic Ocean, Straits of
Florida
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID GENUS
AB The first observation in the North Atlantic Ocean of the deep sea squid Asperoteuthis acanthoderma (family Chiroteuthidae) is reported here from off the coast of Key West, Florida in the Straits of Florida. We describe the morphology of the two nearly complete, but damaged, specimens. A third record is based on photographs of a specimen from off Grand Cayman Island; this specimen was not available for examination. The multiple occurrences of this species, heretofore unknown in the North Atlantic Ocean, within a 10-month period are so unusual that we attempt to hypothesize an explanation for these events. All previously known records are recorded from a few specimens scattered from Hawaii to the Philippines. The present specimens were identified by the following characteristics unique to the species: Y-shaped funnel locking apparatus, sucker ring form and dentition, beak morphology, photophore patch configuration on ventral surface of eyeballs, and numerous small cartilaginous tubercles that cover the mantle, head and the aboral surface of the arms.
C1 [Judkins, Heather] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Ingrao, Debra A.] Mote Marine Lab, Sarasota, FL 34236 USA.
[Roper, Clyde F. E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Judkins, H (reprint author), Univ S Florida, Coll Marine Sci, 140 7th Ave S, St Petersburg, FL 33701 USA.
EM judkins@mail.usf.edu; dingrao@gmail.com; gsquidinc@verizon.net
NR 8
TC 1
Z9 1
U1 0
U2 3
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 162
EP 170
PG 9
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300005
ER
PT J
AU Kornicker, LS
Iliffe, TM
Harrison-Nelson, E
AF Kornicker, Louis S.
Iliffe, Thomas M.
Harrison-Nelson, Elizabeth
TI Ontogeny of Deeveya medix Kornicker, 1990, collected in anchialine and
marine caves in the Bahama Islands (Ostracoda: Halocypridae: Deeveyinae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID GREAT EXUMA ISLAND; CRUSTACEA
AB Four juvenile instars of Deeveya medix (Instars I, II, III, and V) from marine caves and blue holes in the Bahamas are described and illustrated. The ontogeny of the species is compared with that of D. spiralis Kornicker & Iliffe, 1985, and D. bransoni Kornicker & Palmer, 1987 and found to be similar. Criteria are presented for identifying stages of species of Deeveya. Each lamella of the furca of known species of Deeveya bears 3 claws on instar I, 4 on instar II, 5 on instar III, 6 on instar IV, and 7 on instar V and the adult.
C1 [Kornicker, Louis S.; Harrison-Nelson, Elizabeth] Smithsonian Inst, MRC 163, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Iliffe, Thomas M.] Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA.
RP Kornicker, LS (reprint author), Smithsonian Inst, MRC 163, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM kornickl@si.edu; iliffet@tamug.edu; nelsone@si.edu
FU Brian Kakuk and the Bahama Caves Research Foundation; Caribbean Marine
Research Center (CMRC) of the National Oceanic and Atmospheric
Administration (NOAA); National Science Foundation [DEB-0315903,
DEB-9870219]
FX Biological collections from caves on Sweeting's Cay and South Andros
viere carried out aboard the M/V Ocean Explorer during a series of
exploratory and scientific expeditions conducted by Brian Kakuk and the
Bahama Caves Research Foundation. Specimens viere obtained under the
terms of Marine Resource Collection Permits issued by the Bahamas
Department of Fisheries to Brian Kakuk and Thomas Iliffe. This research
was supported by grants from the Caribbean Marine Research Center (CMRC)
of the National Oceanic and Atmospheric Administration (NOAA) and from
the National Science Foundation (DEB-0315903 and DEB-9870219) to T.
Iliffe. We thank Megan Bluhm for inking the drawings, Molly K. Ryan,
Smithsonian Institution, for preparing the map, and Abbie Yorkoff,
Smithsonian Institution, for preparing the manuscript for publication.
NR 10
TC 1
Z9 1
U1 1
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD JUL 30
PY 2009
VL 122
IS 2
BP 171
EP 205
PG 35
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 478WW
UT WOS:000268620300006
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI The Copernicus grave mystery
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Editorial Material
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ginger@cfa.harvard.edu
NR 6
TC 1
Z9 1
U1 0
U2 0
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JUL 28
PY 2009
VL 106
IS 30
BP 12215
EP 12216
DI 10.1073/pnas.0907491106
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 476KV
UT WOS:000268440200003
PM 19622737
ER
PT J
AU Petraglia, M
Clarkson, C
Boivin, N
Haslam, M
Korisettar, R
Chaubey, G
Ditchfield, P
Fuller, D
James, H
Jones, S
Kivisild, T
Koshy, J
Lahr, MM
Metspalu, M
Roberts, R
Arnold, L
AF Petraglia, Michael
Clarkson, Christopher
Boivin, Nicole
Haslam, Michael
Korisettar, Ravi
Chaubey, Gyaneshwer
Ditchfield, Peter
Fuller, Dorian
James, Hannah
Jones, Sacha
Kivisild, Toomas
Koshy, Jinu
Lahr, Marta Mirazon
Metspalu, Mait
Roberts, Richard
Arnold, Lee
TI Population increase and environmental deterioration correspond with
microlithic innovations in South Asia ca. 35,000 years ago
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE archaeology; environment; genetics; lithic technology
ID MTDNA VARIATION; ARABIAN SEA; RECORD; EAST; COLONIZATION; REVOLUTION;
AUSTRALIA; EVOLUTION; BEHAVIOR; GENOMES
AB Genetic studies of South Asia's population history have led to postulations of a significant and early population expansion in the subcontinent, dating to sometime in the Late Pleistocene. We evaluate this argument, based on new mtDNA analyses, and find evidence for significant demographic transition in the subcontinent, dating to 35-28 ka. We then examine the paleoenvironmental and, particularly, archaeological records for this time period and note that this putative demographic event coincides with a period of ecological and technological change in South Asia. We document the development of a new diminutive stone blade (microlithic) technology beginning at 35-30 ka, the first time that the precocity of this transition has been recognized across the subcontinent. We argue that the transition to microlithic technology may relate to changes in subsistence practices, as increasingly large and probably fragmented populations exploited resources in contracting favorable ecological zones just before the onset of full glacial conditions.
C1 [Petraglia, Michael; Boivin, Nicole; Haslam, Michael; Ditchfield, Peter] Univ Oxford, Archaeol & Hist Art Res Lab, Oxford OX1 3QY, England.
[Petraglia, Michael] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
[Clarkson, Christopher] Univ Queensland, Sch Social Sci, St Lucia, Qld 4072, Australia.
[Korisettar, Ravi; Koshy, Jinu] Karnatak Univ, Dept Hist & Archaeol, Dharwad 580003, Karnataka, India.
[Chaubey, Gyaneshwer] Ctr Cellular & Mol Biol, Hyderabad 500007, Andhra Pradesh, India.
[Chaubey, Gyaneshwer; Metspalu, Mait] Univ Tartu, Dept Evolut Biol, Inst Mol & Cell Biol, EE-51010 Tartu, Estonia.
[Chaubey, Gyaneshwer; Metspalu, Mait] Estonian Bioctr, EE-51010 Tartu, Estonia.
[Fuller, Dorian] UCL, Inst Archaeol, London WC1H 0PY, England.
[James, Hannah; Kivisild, Toomas; Lahr, Marta Mirazon] Univ Cambridge, Leverhulme Ctr Human Evolutionary Studies, Cambridge CB2 1QH, England.
[Jones, Sacha] Univ Cambridge, McDonald Inst Archaeol Res, Cambridge CB2 3ER, England.
[Roberts, Richard; Arnold, Lee] Univ Wollongong, GeoQuEST Res Ctr, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia.
RP Petraglia, M (reprint author), Univ Oxford, Archaeol & Hist Art Res Lab, Oxford OX1 3QY, England.
EM michael.petraglia@rlaha.ox.ac.uk
RI Fuller, Dorian/C-1908-2008; Chaubey, Gyaneshwer/H-2753-2012; Roberts,
Richard/B-8245-2013; Metspalu, Mait/G-8671-2015;
OI Fuller, Dorian/0000-0002-4859-080X; Chaubey,
Gyaneshwer/0000-0003-2899-3852; Roberts, Richard/0000-0002-0128-4119;
Metspalu, Mait/0000-0003-3099-9161; Clarkson, Chris/0000-0002-8938-8974;
Arnold, Lee/0000-0001-9603-3824; Haslam, Michael/0000-0001-8234-7806
FU British Academy; The Leverhulme Trust; The Leakey Foundation; McDonald
Institute for Archaeological Research; Natural Environmental Research
Council's Environmental Factors in the Chronology of Human Evolution and
Dispersal Program; Natural Environmental Research Council's Arts and
Humanities Research Council Oxford Radiocarbon Accelerator Dating
Service; Australian Research Council; Leakey Trust; Royal
Anthropological Institute
FX We thank P. Mellars for useful discussions. This project was funded by
the British Academy, The Leverhulme Trust, The Leakey Foundation, the
McDonald Institute for Archaeological Research, the Natural
Environmental Research Council's Environmental Factors in the Chronology
of Human Evolution and Dispersal Program, the Natural Environmental
Research Council's Arts and Humanities Research Council Oxford
Radiocarbon Accelerator Dating Service, the Australian Research Council,
the Leakey Trust, and the Royal Anthropological Institute. We thank the
Archaeological Survey of India for permission to conduct fieldwork; the
Smithsonian Institution and the American Institute of American Studies
for assistance; the authorities of Deccan College for access to the
Patne collections; and the participants of the Kurnool project for their
contributions to the excavations and artifact cataloguing.
NR 45
TC 45
Z9 46
U1 4
U2 12
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JUL 28
PY 2009
VL 106
IS 30
BP 12261
EP 12266
DI 10.1073/pnas.0810842106
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 476KV
UT WOS:000268440200013
PM 19620737
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Bautista, M
Beilicke, M
Benbow, W
Bradbury, SM
Buckley, JH
Bugaev, V
Butt, Y
Byrum, K
Cannon, A
Celik, O
Cesarini, A
Chow, YC
Ciupik, L
Cogan, P
Cui, W
Dickherber, R
Fegan, SJ
Finley, JP
Fortin, P
Fortson, L
Furniss, A
Gall, D
Gillanders, GH
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Horan, D
Hui, CM
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kieda, D
Kildea, J
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McCann, A
McCutcheon, M
Millis, J
Moriarty, P
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Petry, D
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Roache, E
Rose, HJ
Schroedter, M
Sembroski, GH
Smith, AW
Swordy, SP
Theiling, M
Toner, JA
Varlotta, A
Vincent, S
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Williams, DA
Wissel, S
Wood, M
Walker, RC
Davies, F
Hardee, PE
Junor, W
Ly, C
Aharonian, F
Akhperjanian, AG
Anton, G
de Almeida, UB
Bazer-Bachi, AR
Becherini, Y
Behera, B
Bernlohr, K
Bochow, A
Boisson, C
Bolmont, J
Borrel, V
Brucker, J
Brun, F
Brun, P
Buhler, R
Bulik, T
Busching, I
Boutelier, T
Chadwick, PM
Charbonnier, A
Chaves, RCG
Cheesebrough, A
Chounet, LM
Clapson, AC
Coignet, G
Dalton, M
Daniel, MK
Davids, ID
Degrange, B
Deil, C
Dickinson, HJ
Djannati-Atai, A
Domainko, W
Drury, LO
Dubois, F
Dubus, G
Dyks, J
Dyrda, M
Egberts, K
Emmanoulopoulos, D
Espigat, P
Farnier, C
Feinstein, F
Fiasson, A
Forster, A
Fontaine, G
Fussling, M
Gabici, S
Gallant, YA
Gerard, L
Gerbig, D
Giebels, B
Glicenstein, JF
Gluck, B
Goret, P
Gohring, D
Hauser, D
Hauser, M
Heinz, S
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hoffmann, A
Hofmann, W
Holleran, M
Hoppe, S
Horns, D
Jacholkowska, A
de Jager, OC
Jahn, C
Jung, I
Katarzynski, K
Katz, U
Kaufmann, S
Kendziorra, E
Kerschhaggl, M
Khangulyan, D
Khelifi, B
Keogh, D
Kluzniak, W
Kneiske, T
Komin, N
Kosack, K
Lamanna, G
Lenain, JP
Lohse, T
Marandon, V
Martin, JM
Martineau-Huynh, O
Marcowith, A
Maurin, D
McComb, TJL
Medina, MC
Moderski, R
Moulin, E
Naumann-Godo, M
de Naurois, M
Nedbal, D
Nekrassov, D
Nicholas, B
Niemiec, J
Nolan, SJ
Ohm, S
Olive, JF
Wilhelmi, ED
Orford, KJ
Ostrowski, M
Panter, M
Arribas, MP
Pedaletti, G
Pelletier, G
Petrucci, PO
Pita, S
Raue, M
Rayner, SM
Renaud, M
Rieger, F
Ripken, J
Rob, L
Rosier-Lees, S
Rowell, G
Rudak, B
Rulten, CB
Ruppel, J
Sahakian, V
Santangelo, A
Schlickeiser, R
Schock, FM
Schroder, R
Schwanke, U
Schwarzburg, S
Schwemmer, S
Shalchi, A
Sikora, M
Skilton, JL
Sol, H
Spangler, D
Stawarz, L
Steenkamp, R
Stegmann, C
Stinzing, F
Superina, G
Szostek, A
Tam, PH
Tavernet, JP
Terrier, R
Tibolla, O
Tluczykont, M
van Eldik, C
Vasileiadis, G
Venter, C
Venter, L
Vialle, JP
Vincent, P
Vivier, M
Volk, HJ
Volpe, F
Wagner, SJ
Ward, M
Zdziarski, AA
Zech, A
Anderhub, H
Antonelli, LA
Antoranz, P
Backes, M
Baixeras, C
Balestra, S
Barrio, JA
Bastieri, D
Gonzlez, JB
Becker, JK
Bednarek, W
Berger, K
Bernardini, E
Biland, A
Bock, RK
Bonnoli, G
Bordas, P
Tridon, DB
Bosch-Ramon, V
Bose, D
Braun, I
Bretz, T
Britvitch, I
Camara, M
Carmona, E
Commichau, S
Contreras, JL
Cortina, J
Costado, MT
Covino, S
Curtef, V
Dazzi, F
De Angelis, A
Del Pozo, ED
Mendez, CD
De los Reyes, R
De Lotto, B
De Maria, M
De Sabata, F
Dominguez, A
Dorner, D
Doro, M
Elsaesser, D
Errando, M
Ferenc, D
Fernndez, E
Firpo, R
Fonseca, MV
Font, L
Galante, N
Lopez, RJG
Garczarczyk, M
Gaug, M
Goebel, F
Hadasch, D
Hayashida, M
Herrero, A
Hildebrand, D
Hohne-Monch, D
Hose, J
Hsu, CC
Jogler, T
Kranich, D
La Barbera, A
Laille, A
Leonardo, E
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lorenz, E
Majumdar, P
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Mariotti, M
Martinez, M
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Miyamoto, H
Moldon, J
Moles, M
Moralejo, A
Nieto, D
Nilsson, K
Ninkovic, J
Oya, I
Paoletti, R
Paredes, JM
Pasanen, M
Pascoli, D
Pauss, F
Pegna, RG
Perez-Torres, MA
Persic, M
Peruzzo, L
Prada, F
Prandini, E
Puchades, N
Reichardt, I
Rhode, W
Ribo, M
Rico, J
Rissi, M
Robert, A
Rugamer, S
Saggion, A
Saito, TY
Salvati, M
Sanchez-Conde, M
Satalecka, K
Scalzotto, V
Scapin, V
Schweizer, T
Shayduk, M
Shore, SN
Sidro, N
Sierpowska-Bartosik, A
Sillanpaa, A
Sitarek, J
Sobczynska, D
Spanier, F
Stamerra, A
Stark, LS
Takalo, L
Tavecchio, F
Temnikov, P
Tescaro, D
Teshima, M
Torres, DF
Turini, N
Vankov, H
Wagner, RM
Zabalza, V
Zandanel, F
Zanin, R
Zapatero, J
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Bautista, M.
Beilicke, M.
Benbow, W.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Butt, Y.
Byrum, K.
Cannon, A.
Celik, O.
Cesarini, A.
Chow, Y. C.
Ciupik, L.
Cogan, P.
Cui, W.
Dickherber, R.
Fegan, S. J.
Finley, J. P.
Fortin, P.
Fortson, L.
Furniss, A.
Gall, D.
Gillanders, G. H.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Horan, D.
Hui, C. M.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kieda, D.
Kildea, J.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McCann, A.
McCutcheon, M.
Millis, J.
Moriarty, P.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Petry, D.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Roache, E.
Rose, H. J.
Schroedter, M.
Sembroski, G. H.
Smith, A. W.
Swordy, S. P.
Theiling, M.
Toner, J. A.
Varlotta, A.
Vincent, S.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Williams, D. A.
Wissel, S.
Wood, M.
Walker, R. C.
Davies, F.
Hardee, P. E.
Junor, W.
Ly, C.
Aharonian, F.
Akhperjanian, A. G.
Anton, G.
de Almeida, U. Barres
Bazer-Bachi, A. R.
Becherini, Y.
Behera, B.
Bernloehr, K.
Bochow, A.
Boisson, C.
Bolmont, J.
Borrel, V.
Brucker, J.
Brun, F.
Brun, P.
Buehler, R.
Bulik, T.
Buesching, I.
Boutelier, T.
Chadwick, P. M.
Charbonnier, A.
Chaves, R. C. G.
Cheesebrough, A.
Chounet, L. -M.
Clapson, A. C.
Coignet, G.
Dalton, M.
Daniel, M. K.
Davids, I. D.
Degrange, B.
Deil, C.
Dickinson, H. J.
Djannati-Atai, A.
Domainko, W.
Drury, L. O'C
Dubois, F.
Dubus, G.
Dyks, J.
Dyrda, M.
Egberts, K.
Emmanoulopoulos, D.
Espigat, P.
Farnier, C.
Feinstein, F.
Fiasson, A.
Foerster, A.
Fontaine, G.
Fuessling, M.
Gabici, S.
Gallant, Y. A.
Gerard, L.
Gerbig, D.
Giebels, B.
Glicenstein, J. F.
Glueck, B.
Goret, P.
Goehring, D.
Hauser, D.
Hauser, M.
Heinz, S.
Heinzelmann, G.
Henri, G.
Hermann, G.
Hinton, J. A.
Hoffmann, A.
Hofmann, W.
Holleran, M.
Hoppe, S.
Horns, D.
Jacholkowska, A.
de Jager, O. C.
Jahn, C.
Jung, I.
Katarzynski, K.
Katz, U.
Kaufmann, S.
Kendziorra, E.
Kerschhaggl, M.
Khangulyan, D.
Khelifi, B.
Keogh, D.
Kluzniak, W.
Kneiske, T.
Komin, Nu.
Kosack, K.
Lamanna, G.
Lenain, J. -P.
Lohse, T.
Marandon, V.
Martin, J. M.
Martineau-Huynh, O.
Marcowith, A.
Maurin, D.
McComb, T. J. L.
Medina, M. C.
Moderski, R.
Moulin, E.
Naumann-Godo, M.
de Naurois, M.
Nedbal, D.
Nekrassov, D.
Nicholas, B.
Niemiec, J.
Nolan, S. J.
Ohm, S.
Olive, J. -F.
Wilhelmi, E. de Ona
Orford, K. J.
Ostrowski, M.
Panter, M.
Arribas, M. Paz
Pedaletti, G.
Pelletier, G.
Petrucci, P. -O.
Pita, S.
Raue, M.
Rayner, S. M.
Renaud, M.
Rieger, F.
Ripken, J.
Rob, L.
Rosier-Lees, S.
Rowell, G.
Rudak, B.
Rulten, C. B.
Ruppel, J.
Sahakian, V.
Santangelo, A.
Schlickeiser, R.
Schoeck, F. M.
Schroeder, R.
Schwanke, U.
Schwarzburg, S.
Schwemmer, S.
Shalchi, A.
Sikora, M.
Skilton, J. L.
Sol, H.
Spangler, D.
Stawarz, L.
Steenkamp, R.
Stegmann, C.
Stinzing, F.
Superina, G.
Szostek, A.
Tam, P. H.
Tavernet, J. -P.
Terrier, R.
Tibolla, O.
Tluczykont, M.
van Eldik, C.
Vasileiadis, G.
Venter, C.
Venter, L.
Vialle, J. P.
Vincent, P.
Vivier, M.
Voelk, H. J.
Volpe, F.
Wagner, S. J.
Ward, M.
Zdziarski, A. A.
Zech, A.
Anderhub, H.
Antonelli, L. A.
Antoranz, P.
Backes, M.
Baixeras, C.
Balestra, S.
Barrio, J. A.
Bastieri, D.
Gonzlez, J. Becerra
Becker, J. K.
Bednarek, W.
Berger, K.
Bernardini, E.
Biland, A.
Bock, R. K.
Bonnoli, G.
Bordas, P.
Tridon, D. Borla
Bosch-Ramon, V.
Bose, D.
Braun, I.
Bretz, T.
Britvitch, I.
Camara, M.
Carmona, E.
Commichau, S.
Contreras, J. L.
Cortina, J.
Costado, M. T.
Covino, S.
Curtef, V.
Dazzi, F.
De Angelis, A.
Del Pozo, E. De Cea
Mendez, C. Delgado
De los Reyes, R.
De Lotto, B.
De Maria, M.
De Sabata, F.
Dominguez, A.
Dorner, D.
Doro, M.
Elsaesser, D.
Errando, M.
Ferenc, D.
Fernndez, E.
Firpo, R.
Fonseca, M. V.
Font, L.
Galante, N.
Lopez, R. J. Garcia
Garczarczyk, M.
Gaug, M.
Goebel, F.
Hadasch, D.
Hayashida, M.
Herrero, A.
Hildebrand, D.
Hoehne-Moench, D.
Hose, J.
Hsu, C. C.
Jogler, T.
Kranich, D.
La Barbera, A.
Laille, A.
Leonardo, E.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lorenz, E.
Majumdar, P.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Mariotti, M.
Martinez, M.
Mazin, D.
Meucci, M.
Miranda, J. M.
Mirzoyan, R.
Miyamoto, H.
Moldon, J.
Moles, M.
Moralejo, A.
Nieto, D.
Nilsson, K.
Ninkovic, J.
Oya, I.
Paoletti, R.
Paredes, J. M.
Pasanen, M.
Pascoli, D.
Pauss, F.
Pegna, R. G.
Perez-Torres, M. A.
Persic, M.
Peruzzo, L.
Prada, F.
Prandini, E.
Puchades, N.
Reichardt, I.
Rhode, W.
Ribo, M.
Rico, J.
Rissi, M.
Robert, A.
Ruegamer, S.
Saggion, A.
Saito, T. Y.
Salvati, M.
Sanchez-Conde, M.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schweizer, T.
Shayduk, M.
Shore, S. N.
Sidro, N.
Sierpowska-Bartosik, A.
Sillanpaa, A.
Sitarek, J.
Sobczynska, D.
Spanier, F.
Stamerra, A.
Stark, L. S.
Takalo, L.
Tavecchio, F.
Temnikov, P.
Tescaro, D.
Teshima, M.
Torres, D. F.
Turini, N.
Vankov, H.
Wagner, R. M.
Zabalza, V.
Zandanel, F.
Zanin, R.
Zapatero, J.
CA VERITAS Collaboration
VLBA 43 Ghz M87 Monitoring Team
HESS Collaboration
MAGIC Collaboration
TI Radio Imaging of the Very-High-Energy gamma-Ray Emission Region in the
Central Engine of a Radio Galaxy
SO SCIENCE
LA English
DT Article
ID SUPERMASSIVE BLACK-HOLE; M87 JET; TEV EMISSION; CRAB-NEBULA; INNER JET;
VARIABILITY; TELESCOPE; OUTBURST; NUCLEUS; VERITAS
AB The accretion of matter onto a massive black hole is believed to feed the relativistic plasma jets found in many active galactic nuclei (AGN). Although some AGN accelerate particles to energies exceeding 10(12) electron volts and are bright sources of very-high-energy (VHE) gamma-ray emission, it is not yet known where the VHE emission originates. Here we report on radio and VHE observations of the radio galaxy Messier 87, revealing a period of extremely strong VHE gamma-ray flares accompanied by a strong increase of the radio flux from its nucleus. These results imply that charged particles are accelerated to very high energies in the immediate vicinity of the black hole.
C1 [Acciari, V. A.; Benbow, W.; Kildea, J.; Perkins, J. S.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.; Holder, J.; Roache, E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Butt, Y.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Fortin, P.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
[Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Petry, D.] European So Observ, D-85748 Garching, Germany.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Walker, R. C.; Davies, F.] NRAO, Socorro, NM 87801 USA.
[Davies, F.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Hardee, P. E.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Junor, W.] Los Alamos Natl Lab, MS D436, ISR 2, Los Alamos, NM USA.
[Ly, C.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA.
[Aharonian, F.; Bernloehr, K.; Bochow, A.; Buehler, R.; Chaves, R. C. G.; Clapson, A. C.; Deil, C.; Domainko, W.; Egberts, K.; Hoffmann, A.; Hofmann, W.; Hoppe, S.; Khangulyan, D.; Kosack, K.; Nekrassov, D.; Ohm, S.; Panter, M.; Rieger, F.; Tibolla, O.; van Eldik, C.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia.
[Bazer-Bachi, A. R.; Borrel, V.; Olive, J. -F.] Ctr Etud Spatiale Rayonnements, CNRS, UPS, F-31029 Toulouse 4, France.
[Horns, D.; Kneiske, T.; Ripken, J.; Tluczykont, M.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[Bernloehr, K.; Dalton, M.; Fuessling, M.; Kerschhaggl, M.; Lohse, T.; Arribas, M. Paz; Schwanke, U.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Boisson, C.; Lenain, J. -P.; Martin, J. M.; Medina, M. C.; Sol, H.; Venter, L.] Univ Paris Diderot, CNRS, Observ Paris, Lab Univers & Theories, F-92190 Meudon, France.
[Brun, F.; Glicenstein, J. F.; Goret, P.; Komin, Nu.; Moulin, E.; Vivier, M.] Commissariat Energie Atom CE Saclay, Inst Rech Lois Fondamentales Univers, Direct Sci Mat, F-91191 Gif Sur Yvette, France.
[de Almeida, U. Barres; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Dickinson, H. J.; Keogh, D.; McComb, T. J. L.; Nolan, S. J.; Orford, K. J.; Rulten, C. B.; Spangler, D.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Buesching, I.; Davids, I. D.; de Jager, O. C.; Venter, C.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa.
[Chounet, L. -M.; Degrange, B.; Fontaine, G.; Giebels, B.; Khelifi, B.; Naumann-Godo, M.; Superina, G.; Volpe, F.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Coignet, G.; Dubois, F.; Lamanna, G.; Rosier-Lees, S.; Vialle, J. P.] Lab Annecy Le Vieux Phys Particules, CNRS, IN2P3, F-74941 Annecy Le Vieux, France.
[Becherini, Y.; Djannati-Atai, A.; Gerard, L.; Marandon, V.; Wilhelmi, E. de Ona; Pita, S.; Terrier, R.] Univ Paris 07, CNRS, Observ Paris, CEA,UMR 7164, F-75205 Paris 13, France.
[Aharonian, F.; Drury, L. O'C; Gabici, S.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Behera, B.; Emmanoulopoulos, D.; Espigat, P.; Gallant, Y. A.; Hauser, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hoffmann, A.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Pedaletti, G.; Pelletier, G.; Raue, M.; Rayner, S. M.; Renaud, M.; Rieger, F.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Tam, P. H.; Tibolla, O.; Wagner, S. J.; Ward, M.; Zdziarski, A. A.; Zech, A.; Anderhub, H.] Univ Heidelberg, D-69117 Heidelberg, Germany.
[Farnier, C.; Feinstein, F.; Fiasson, A.; Gallant, Y. A.; Marcowith, A.; Vasileiadis, G.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, F-34095 Montpellier 5, France.
[Anton, G.; Brucker, J.; Glueck, B.; Goehring, D.; Jahn, C.; Jung, I.; Katz, U.; Schoeck, F. M.; Stegmann, C.; Stinzing, F.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany.
[Boutelier, T.; Dubus, G.; Pelletier, G.; Petrucci, P. -O.; Szostek, A.] Univ Grenoble 1, CNRS, Astrophys Lab, Inst Natl Sci Univers, F-38041 Grenoble 9, France.
[Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Bolmont, J.; Brun, F.; Charbonnier, A.; Jacholkowska, A.; Martineau-Huynh, O.; Maurin, D.; de Naurois, M.; Tavernet, J. -P.; Vincent, P.] Univ Paris 07, CNRS, Univ Paris 06, Lab Phys Nucl & Hautes,IN2P3, F-75252 Paris 5, France.
[Nedbal, D.; Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague, Czech Republic.
[Gerbig, D.; Kluzniak, W.; Ruppel, J.; Schlickeiser, R.; Schroeder, R.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany.
[Davids, I. D.; Steenkamp, R.] Univ Namibia, Windhoek, Namibia.
[Ostrowski, M.; Stawarz, L.; Szostek, A.] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland.
[Bulik, T.; Dyks, J.; Moderski, R.; Rudak, B.; Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Hinton, J. A.; Skilton, J. L.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Nicholas, B.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Katarzynski, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Baixeras, C.; Font, L.; Hadasch, D.; Robert, A.; Zapatero, J.] Univ Autonoma Barcelona, E-08193 Barcelona, Spain.
[Bastieri, D.; Bock, R. K.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Pascoli, D.; Saggion, A.; Scalzotto, V.] Univ Padua, I-35131 Padua, Italy.
[Gonzlez, J. Becerra; Costado, M. T.; Mendez, C. Delgado; Lopez, R. J. Garcia; Gaug, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Bednarek, W.; Berger, K.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; Majumdar, P.; Satalecka, K.] DESY, D-15738 Zeuthen, Germany.
[Bock, R. K.; Tridon, D. Borla; Carmona, E.; Galante, N.; Goebel, F.; Hayashida, M.; Hsu, C. C.; Jogler, T.; Lorenz, E.; Mirzoyan, R.; Miyamoto, H.; Ninkovic, J.; Saito, T. Y.; Schweizer, T.; Shayduk, M.; Sitarek, J.; Teshima, M.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Bonnoli, G.; Leonardo, E.; Paoletti, R.; Pegna, R. G.; Stamerra, A.; Turini, N.] Univ Siena, I-53100 Siena, Italy.
[Bordas, P.; Bosch-Ramon, V.; Moldon, J.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona, IEEC, Inst Ciencias Cosmos, E-08028 Barcelona, Spain.
[Bretz, T.; Elsaesser, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Cortina, J.; Errando, M.; Fernndez, E.; Firpo, R.; Garczarczyk, M.; Martinez, M.; Moralejo, A.; Puchades, N.; Reichardt, I.; Rico, J.; Sidro, N.; Tescaro, D.; Zanin, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Costado, M. T.; Lopez, R. J. Garcia] Dept Astrofis, E-38206 Tenerife, Spain.
[Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Scapin, V.] Univ Udine, I-33100 Udine, Italy.
[Del Pozo, E. De Cea; Sierpowska-Bartosik, A.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Dominguez, A.; Moles, M.; Perez-Torres, M. A.; Sanchez-Conde, M.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Ferenc, D.; Laille, A.] Univ Calif Davis, Davis, CA 95616 USA.
[Lindfors, E.; Nilsson, K.; Pasanen, M.; Sillanpaa, A.; Takalo, L.] Turku Univ, Tuorla Observ, FI-21500 Piikkio, Finland.
[Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Persic, M.] INAF, Osservatorio Astron, I-34143 Trieste, Italy.
[Rico, J.; Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Bastieri, D.; Bock, R. K.; Doro, M.; Lombardi, S.; Paoletti, R.; Persic, M.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Bonnoli, G.; Leonardo, E.; Paoletti, R.; Stamerra, A.; Turini, N.] Ist Nazl Fis Nucl, I-53100 Siena, Italy.
[Dazzi, F.; De Angelis, A.; De Lotto, B.; De Maria, M.; De Sabata, F.; Longo, F.; Mankuzhiyil, N.; Scapin, V.] Ist Nazl Fis Nucl, I-33100 Udine, Italy.
[Persic, M.] Ist Nazl Fis Nucl, I-34143 Trieste, Italy.
[Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy.
RP Beilicke, M (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
EM beilicke@physics.wustl.edu; krawcz@wuphys.wustl.edu;
cwalker@aoc.nrao.edu; phardee@bama.ua.edu; martin.raue@mpi-hd.mpg.de;
mazin@ifae.es; robert.wagner@mpp.mpg.de
RI Horns, Dieter/C-9727-2011; GAug, Markus/L-2340-2014; Venter,
Christo/E-6884-2011; Braun, Isabel/C-9373-2012; Mannheim,
Karl/F-6705-2012; Doro, Michele/F-9458-2012; van Eldik,
Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Tjus, Julia/G-8145-2012;
Fontaine, Gerard/D-6420-2014; Contreras Gonzalez, Jose Luis/K-7255-2014;
Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Font,
Lluis/L-4197-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo,
Marc/B-3579-2015; Katarzynski, Krzysztof/G-4528-2014; Antoranz,
Pedro/H-5095-2015; Anton, Gisela/C-4840-2013; Fonseca Gonzalez, Maria
Victoria/I-2004-2015; Delgado, Carlos/K-7587-2014; Nieto,
Daniel/J-7250-2015; Maneva, Galina/L-7120-2016; Backes,
Michael/N-5126-2016; Torres, Diego/O-9422-2016; Reichardt,
Ignasi/P-7478-2016; Temnikov, Petar/L-6999-2016; Drury,
Luke/B-1916-2017; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017;
Daniel, Michael/A-2903-2010;
OI GAug, Markus/0000-0001-8442-7877; Venter, Christo/0000-0002-2666-4812;
Braun, Isabel/0000-0002-9389-0502; Doro, Michele/0000-0001-9104-3214;
van Eldik, Christopher/0000-0001-9669-645X; Katz,
Uli/0000-0002-7063-4418; Contreras Gonzalez, Jose
Luis/0000-0001-7282-2394; Rico, Javier/0000-0003-4137-1134; Font,
Lluis/0000-0003-2109-5961; Moralejo Olaizola,
Abelardo/0000-0002-1344-9080; Antoranz, Pedro/0000-0002-3015-3601;
Anton, Gisela/0000-0003-2039-4724; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; Delgado, Carlos/0000-0002-7014-4101;
Nieto, Daniel/0000-0003-3343-0755; Backes, Michael/0000-0002-9326-6400;
Torres, Diego/0000-0002-1522-9065; Reichardt,
Ignasi/0000-0003-3694-3820; Temnikov, Petar/0000-0002-9559-3384; Drury,
Luke/0000-0002-9257-2270; Barrio, Juan/0000-0002-0965-0259; Cortina,
Juan/0000-0003-4576-0452; leonardo, elvira/0000-0003-0271-7673;
Chadwick, Paula/0000-0002-1468-2685; Costado, M.
Teresa/0000-0002-2672-4061; Kneiske, Tanja M./0000-0002-3210-6200; LA
BARBERA, ANTONINO/0000-0002-5880-8913; Cui, Wei/0000-0002-6324-5772;
Daniel, Michael/0000-0002-8053-7910; Cesarini,
Andrea/0000-0002-8611-8610; de los Reyes Lopez,
Raquel/0000-0003-0485-9552; De Lotto, Barbara/0000-0003-3624-4480; Hsu,
Ching-Cheng/0000-0001-9406-2023; De Angelis,
Alessandro/0000-0002-3288-2517; Persic, Massimo/0000-0003-1853-4900
FU ETH [TH 34/043]; Polish MniSzW [N N203 390834]; Young Investigators
Program of the Helmholtz Gemeinschaft; U.S. Department of Energy; NSF;
Smithsonian Institution; Natural Sciences and Engineering Research
Council of Canada; Science Foundation Ireland; STFC, U.K
FX This work was also supported by ETH research grant TH 34/043, the Polish
MniSzW grant N N203 390834, and the Young Investigators Program of the
Helmholtz Gemeinschaft. VERITAS: This research is supported by grants
from the U.S. Department of Energy, NSF, the Smithsonian Institution,
the Natural Sciences and Engineering Research Council of Canada, Science
Foundation Ireland, and the STFC in the U.K. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and the collaborating institutions in the
construction and operation of the instrument. VLBA: The Very Long
Baseline Array is operated by the National Radio Astronomy Observatory,
a facility of NSF, operated under cooperative agreement by Associated
Universities, Inc.
NR 31
TC 115
Z9 115
U1 2
U2 17
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUL 24
PY 2009
VL 325
IS 5939
BP 444
EP 448
DI 10.1126/science.1175406
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 474AR
UT WOS:000268255100048
ER
PT J
AU Sues, HD
Averianov, A
AF Sues, Hans-Dieter
Averianov, Alexander
TI A new basal hadrosauroid dinosaur from the Late Cretaceous of Uzbekistan
and the early radiation of duck-billed dinosaurs
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE Dinosauria; Hadrosauroidea; Cretaceous; Asia; radiation;
palaeobiogeography
ID IREN DABASU FORMATION; REPUBLIC-OF-CHINA; INNER-MONGOLIA; ORNITHISCHIA;
EVOLUTION; PHYLOGENY; BEARING
AB Levnesovia transoxiana gen. et sp. nov., from the Late Cretaceous (Middle-Late Turonian) of Uzbekistan, is the oldest well-documented taxon referable to Hadrosauroidea sensu Godefroit et al. It differs from a somewhat younger and closely related Bactrosaurus from Inner Mongolia (China) by a tall sagittal crest on the parietals and the absence of club-shaped dorsal neural spines in adult specimens. Levnesovia, Bactrosaurus and possibly Gilmoreosaurus represent the earliest radiation of Hadrosauroidea, which took place during the Cenomanian-Turonian and possibly in North America. The second, Santonian-age radiation of Hadrosauroidea included Aralosaurus, Hadrosauridae and lineages leading to Tanius (Campanian) and Telmatosaurus (Maastrichtian). Hadrosauridae appears to be monophyletic, but Hadrosaurinae and Lambeosaurinae originated in North America and Asia, respectively.
C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, MRC 106, Washington, DC 20013 USA.
[Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia.
RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 106, POB 37012, Washington, DC 20013 USA.
EM suesh@si.edu
RI Averianov, Alexander/M-8490-2013
OI Averianov, Alexander/0000-0001-5948-0799
FU National Science Foundation [EAR-9804771, 0207004]; National Geographic
Society [5901-97, 6281-98]; US Civilian Research and Development
Foundation [RUB1-2860-ST-07]
FX We thank three anonymous reviewers for their helpful suggestions on a
draft of the manuscript. Fieldwork and research were supported by grants
from the National Science Foundation (EAR-9804771 and 0207004) and
National Geographic Society (5901-97 and 6281-98) to J. D. Archibald
(San Diego State University) and H.-D.S. as well as US Civilian Research
and Development Foundation grant RUB1-2860-ST-07 to A. A. and J. D.
Archibald.
NR 38
TC 39
Z9 42
U1 0
U2 8
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P R SOC B
JI Proc. R. Soc. B-Biol. Sci.
PD JUL 22
PY 2009
VL 276
IS 1667
BP 2549
EP 2555
DI 10.1098/rspb.2009.0229
PG 7
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 461PP
UT WOS:000267280900005
PM 19386651
ER
PT J
AU Himler, AG
Caldera, EJ
Baer, BC
Fernandez-Marin, H
Mueller, UG
AF Himler, Anna G.
Caldera, Eric J.
Baer, Boris C.
Fernandez-Marin, Hermogenes
Mueller, Ulrich G.
TI No sex in fungus-farming ants or their crops
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE asexual; fungus-growing ants; symbiosis; Mycocepurus smithii; Wolbachia;
thelytoky
ID MYCOCEPURUS-SMITHII; BACTERIAL SYMBIONT; WOLBACHIA STRAINS; NEST
ARCHITECTURE; ASEXUAL LINEAGES; GENE-SEQUENCES; GROWING ANTS;
PARTHENOGENESIS; EVOLUTION; HYMENOPTERA
AB Asexual reproduction imposes evolutionary handicaps on asexual species, rendering them prone to extinction, because asexual reproduction generates novel genotypes and purges deleterious mutations at lower rates than sexual reproduction. Here, we report the first case of complete asexuality in ants, the fungus-growing ant Mycocepurus smithii, where queens reproduce asexually but workers are sterile, which is doubly enigmatic because the clonal colonies of M. smithii also depend on clonal fungi for food. Degenerate female mating anatomy, extensive field and laboratory surveys, and DNA fingerprinting implicate complete asexuality in this widespread ant species. Maternally inherited bacteria (e. g. Wolbachia, Cardinium) and the fungal cultivars can be ruled out as agents inducing asexuality. M. smithii societies of clonal females provide a unique system to test theories of parent-offspring conflict and reproductive policing in social insects. Asexuality of both ant farmer and fungal crop challenges traditional views proposing that sexual farmer ants outpace coevolving sexual crop pathogens, and thus compensate for vulnerabilities of their asexual crops. Either the double asexuality of both farmer and crop may permit the host to fully exploit advantages of asexuality for unknown reasons or frequent switching between crops (symbiont reassociation) generates novel ant-fungus combinations, which may compensate for any evolutionary handicaps of asexuality in M. smithii.
C1 [Himler, Anna G.; Caldera, Eric J.; Mueller, Ulrich G.] Univ Texas Austin, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA.
[Baer, Boris C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Baer, Boris C.] Sch Anim Biol, Crawley, WA 6009, Australia.
[Fernandez-Marin, Hermogenes] Univ Puerto Rico, Dept Biol, San Juan, PR 00901 USA.
[Fernandez-Marin, Hermogenes; Mueller, Ulrich G.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Himler, AG (reprint author), Univ Texas Austin, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA.
EM ahimler@email.arizona.edu
RI Baer, Boris/F-5301-2011
OI Baer, Boris/0000-0002-1136-5967
FU NSF [DEB-0206372, DEB-9983879, DEB-0110073]; Section of Integrative
Biology at UT Austin; Swiss National Science Foundation [PA00A-104991];
Danish Natural Science Research Council
FX This work was supported by the NSF to AGH (DEB-0206372) and UGM
(DEB-9983879, DEB-0110073) and the Section of Integrative Biology at UT
Austin to AGH. B. C. B. was supported by the Swiss National Science
Foundation (PA00A-104991) and the Danish Natural Science Research
Council. We thank the Smithsonian Tropical Research Institute and the
Autoridad Nacional del Ambiente of the Republic of Panama for collecting
permits; T. Wenseleers, K. Stanger-Hall and S. Perlman for Wolbachia and
Cardinium controls; and B. Brandao for loaning Mycocepurus specimens
from the Museu de Zoologia, Brazil. The authors are grateful to R.
Adams, C. Currie, N. Gerardo, R. Koshy and A. Little for research
assistance; C. Rabeling for sharing unpublished collection information;
M. Florance and D. Hall for assistance with statistical analyses; and P.
Abbot, N. Gerardo, B. Klein, C. Rabeling and A. Woods for helpful
comments on the manuscript.
NR 41
TC 31
Z9 32
U1 0
U2 20
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P R SOC B
JI Proc. R. Soc. B-Biol. Sci.
PD JUL 22
PY 2009
VL 276
IS 1667
BP 2611
EP 2616
DI 10.1098/rspb.2009.0313
PG 6
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 461PP
UT WOS:000267280900013
PM 19369264
ER
PT J
AU Li, ZY
Wang, QD
Wakker, BP
AF Li, Zhiyuan
Wang, Q. Daniel
Wakker, Bart P.
TI M31*and its circumnuclear environment
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: general; galaxies: individual: M31; galaxies: spiral; X-rays:
general
ID EARLY-TYPE GALAXIES; SUPERMASSIVE BLACK-HOLE; O-VI ABSORPTION; X-RAY
BINARIES; ELLIPTIC GALAXIES; ANDROMEDA GALAXY; STAR-FORMATION;
IONIZED-GAS; HOT GAS; STELLAR POPULATIONS
AB We present a multiwavelength investigation of the circumnuclear environment of the Andromeda galaxy (M31), utilizing archival Chandra, FUSE, GALEX, HST and Spitzer data as well as ground-based observations. Based on the Chandra/ACIS data, we tightly constrain the X-ray luminosity of M31*, the central supermassive black hole (SMBH) of the galaxy, to be L(0.3-7 keV) less than or similar to 1.2 x 10(36) erg s(-1), approximately one part per 10(10) of the Eddington luminosity. From the diffuse X-ray emission, we characterize the circumnuclear hot gas with a temperature of similar to 0.3 keV and a density of similar to 0.1 cm(-3). In the absence of an active SMBH and recent star formation, the most likely heating source for the hot gas is Type Ia supernovae (SNe). The presence of cooler, dusty gas residing in a nuclear spiral has long been known in terms of optical line emission and extinction. We further reveal the infrared emission of the nuclear spiral and evaluate the relative importance of various possible ionizing sources. We show evidence for interaction between the nuclear spiral and the hot gas, probably via thermal evaporation. This mechanism lends natural understandings to (1) the inactivity of M31*, in spite of a probably continuous supply of gas from outer disc regions and (2) the launch of a bulge outflow of hot gas, primarily mass-loaded from the circumnuclear regions. One particular prediction of such a scenario is the presence of gas with intermediate temperatures arising from the conductive interfaces. The FUSE observations do show strong O vi lambda 1032 and lambda 1038 absorption lines against the bulge starlight, but the effective column density, N(O VI) similar to 4 x 10(14) cm(-2), may be attributed to foreground gas located in the bulge and/or the highly inclined disc of M31, leaving the amount of circumnuclear gas with intermediate temperatures largely uncertain. Our study strongly argues that stellar feedback, particularly in the form of energy release from SNe Ia, may play an important role in regulating the evolution of SMBHs and the interstellar medium in galactic bulges.
C1 [Li, Zhiyuan; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Li, Zhiyuan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wakker, Bart P.] Univ Wisconsin, Dept Astron, Madison, WI 53705 USA.
RP Li, ZY (reprint author), Univ Massachusetts, Dept Astron, 710 N Pleasant St, Amherst, MA 01003 USA.
EM zyli@head.cfa.harvard.edu; wqd@astro.umass.edu; wakker@astro.wisc.edu
FU SAO [AR7-8006X]
FX We are indebted to Dr N. Devereux for providing the H alpha image and to
Dr L. Ji for providing the numerical data utilized in Fig. 9. It is a
pleasure to thank Drs D. Calzatti, M. Garcia, Z. Han and L. Ho for
stimulating and helpful discussions. This work is supported by the SAO
grant AR7-8006X.
NR 103
TC 25
Z9 25
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL 21
PY 2009
VL 397
IS 1
BP 148
EP 163
DI 10.1111/j.1365-2966.2009.14918.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482XE
UT WOS:000268923100035
ER
PT J
AU Pedretti, E
Monnier, JD
Lacour, S
Traub, WA
Danchi, WC
Tuthill, PG
Thureau, ND
Millan-Gabet, R
Berger, JP
Lacasse, MG
Schuller, PA
Schloerb, FP
Carleton, NP
AF Pedretti, E.
Monnier, J. D.
Lacour, S.
Traub, W. A.
Danchi, W. C.
Tuthill, P. G.
Thureau, N. D.
Millan-Gabet, R.
Berger, J. -P.
Lacasse, M. G.
Schuller, P. A.
Schloerb, F. P.
Carleton, N. P.
TI Detection of non-radial pulsation and faint companion in the symbiotic
star CH Cyg
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: high angular resolution; techniques: interferometric;
binaries: symbiotic; stars: imaging; stars: individual: CH Cygni
ID GRAVITATIONAL LENSING EXPERIMENT; LONG SECONDARY PERIODS;
LARGE-MAGELLANIC-CLOUD; RED GIANT STARS; IOTA INTERFEROMETRY;
INTEGRATED-OPTICS; LAMBDA-VIRGINIS; MIRA VARIABLES; DUST ENVELOPE; BROWN
DWARF
AB We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 +/- 0.1 D-* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 +/- 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star.
C1 [Monnier, J. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Lacour, S.; Berger, J. -P.] LAOG, Grenoble, France.
[Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Millan-Gabet, R.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA.
[Lacasse, M. G.; Carleton, N. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Schuller, P. A.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Schloerb, F. P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Pedretti, E.; Thureau, N. D.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
RP Pedretti, E (reprint author), Scottish Univ Phys Alliance, Edinburgh, Midlothian, Scotland.
EM ep41@st-and.ac.uk
FU European Community's Sixth Framework Programme through an International
Outgoing Marie-Curie fellowship [OIF - 002990]
FX We acknowledge Leslie Hebb for a useful discussion. We thank Kenneth
Hinkle and Francis Fekel for making available to us their data and
results prior to publication and for many useful discussions and advice.
This research was made possible thanks to a Michelson Postdoctoral
Fellowship and a SUPA advanced fellowship awarded to E. Pedretti. N.
Thureau received research funding from the European Community's Sixth
Framework Programme through an International Outgoing Marie-Curie
fellowship OIF - 002990. The IONIC project is a collaboration among the
Laboratoire d'Astrophysique de Grenoble (LAOG), Laboratoire
d'Electromagnetisme Microondes et Optoelectronique (LEMO), and also
CEA-LETI and IMEP, Grenoble, France. The IONIC project is funded in
France by the Centre National de Recherche Scientifique and Centre
National d'Etudes Spatiales. This research has made use of NASA's
Astrophysics Data System Bibliographic Services and of the simbad. data
base operated at CDS, Strasbourg, France.
NR 63
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
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL 21
PY 2009
VL 397
IS 1
BP 325
EP 334
DI 10.1111/j.1365-2966.2009.14906.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482XE
UT WOS:000268923100048
ER
PT J
AU Kim, DW
Protopapas, P
Alcock, C
Byun, YI
Bianco, FB
AF Kim, Dae-Won
Protopapas, Pavlos
Alcock, Charles
Byun, Yong-Ik
Bianco, Federica B.
TI Detrending time series for astronomical variability surveys
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: miscellaneous; methods: statistical;
surveys
ID AMERICAN OCCULTATION SURVEY; RESOLVED CCD PHOTOMETRY;
CORRELATION-COEFFICIENT; LIGHT CURVES; PLANET; STARS; FIELD; CANDIDATES;
CATALOG; PROJECT
AB We present a detrending algorithm for the removal of trends in time series. Trends in time series could be caused by various systematic and random noise sources such as cloud passages, changes of airmass, telescope vibration, CCD noise or defects of photometry. Those trends undermine the intrinsic signals of stars and should be removed. We determine the trends from subsets of stars that are highly correlated among themselves. These subsets are selected based on a hierarchical tree clustering algorithm. A bottom-up merging algorithm based on the departure from normal distribution in the correlation is developed to identify subsets, which we call clusters. After identification of clusters, we determine a trend per cluster by weighted sum of normalized light curves. We then use quadratic programming to detrend all individual light curves based on these determined trends. Experimental results with synthetic light curves containing artificial trends and events are presented. Results from other detrending methods are also compared. The developed algorithm can be applied to time series for trend removal in both narrow and wide field astronomy.
C1 [Kim, Dae-Won; Protopapas, Pavlos; Alcock, Charles; Bianco, Federica B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kim, Dae-Won; Protopapas, Pavlos] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA.
[Kim, Dae-Won; Byun, Yong-Ik] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
[Bianco, Federica B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dakim@cfa.harvard.edu
FU Korea Research Foundation; FAS Research Computing Group at the Harvard;
[KRF-2007-C00020]
FX This work is supported by the Korea Research Foundation. Y.-I. Byun also
acknowledges the grant of KRF-2007-C00020. We thank R. Reid, R. Dave, G.
Wachman and D. Preston at the Harvard, Initiative in Innovative
Computing (IIC), and A. W. Blocker at the Harvard University Department
of Statistics for comments and suggestions on this paper. We also thank
the Harvard-Smithsonian Center for Astrophysics and IIC for providing
computing facilities and research space. The simulations and the
detrending of data sets in this paper were run on the Odyssey cluster
supported by the FAS Research Computing Group at the Harvard.
NR 48
TC 11
Z9 11
U1 0
U2 4
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL 21
PY 2009
VL 397
IS 1
BP 558
EP 568
DI 10.1111/j.1365-2966.2009.14967.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482XE
UT WOS:000268923100070
ER
PT J
AU Hannikainen, DC
Hunstead, RW
Wu, K
McIntyre, V
Lovell, JEJ
Campbell-Wilson, D
McCollough, ML
Reynolds, J
Tzioumis, AK
AF Hannikainen, D. C.
Hunstead, R. W.
Wu, K.
McIntyre, V.
Lovell, J. E. J.
Campbell-Wilson, D.
McCollough, M. L.
Reynolds, J.
Tzioumis, A. K.
TI Revisiting the relativistic ejection event in XTE J1550-564 during the
1998 outburst
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: XTE J1550-564; radio continuum: stars; radio lines:
stars; X-rays: binaries
ID X-RAY-EMISSION; BLACK-HOLE; OPTICAL OBSERVATIONS; GRO J1655-40;
LARGE-SCALE; HIGH STATE; JETS; XTE-J1550-564; BEHAVIOR; VARIABILITY
AB We revisit the discovery outburst of the X-ray transient XTE J1550-564 during which relativistic jets were observed in 1998 September, and review the radio images obtained with the Australian Long Baseline Array, and light curves obtained with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. Based on Hi spectra, we constrain the source distance to between 3.3 and 4.9 kpc. The radio images, taken some 2 d apart, show the evolution of an ejection event. The apparent separation velocity of the two outermost ejecta is at least 1.3c and may be as large as 1.9c; when relativistic effects are taken into account, the inferred true velocity is >= 0.8c. The flux densities appear to peak simultaneously during the outburst, with a rather flat (although still optically thin) spectral index of -0.2.
C1 [Hannikainen, D. C.] TKK, Metsahovi Radio Observ, FI-02540 Kylmala, Finland.
[Hunstead, R. W.; Campbell-Wilson, D.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Wu, K.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[McIntyre, V.; Reynolds, J.; Tzioumis, A. K.] CSIRO, ATNF, Epping, NSW 1710, Australia.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[McCollough, M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hannikainen, DC (reprint author), TKK, Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland.
EM diana@kurp.hut.fi
FU Australian Research Council; Commonwealth of Australia for operation as
a National Facility managed by CSIRO; Academy of Finland [212656]
FX The authors thank Robert Braun and Jim Caswell for helpful discussions
on the distance to XTE J1550-564. MOST is operated by the University of
Sydney and supported by grants from the Australian Research Council. The
ATCA and the Mopra Telescope are part of the Australia Telescope which
is funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. We thank the staff of both the University of
Tasmania and the Canberra Deep Space Communications Complex,
Tidbinbilla. DCH gratefully acknowledges the Academy of Finland for a
Fellowship and project number 212656.
NR 41
TC 18
Z9 18
U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL 21
PY 2009
VL 397
IS 1
BP 569
EP 576
DI 10.1111/j.1365-2966.2009.14997.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482XE
UT WOS:000268923100071
ER
PT J
AU Soleri, P
Heinz, S
Fender, R
Wijnands, R
Tudose, V
Altamirano, D
Jonker, PG
van der Klis, M
Kuiper, L
Kaiser, C
Casella, P
AF Soleri, P.
Heinz, S.
Fender, R.
Wijnands, R.
Tudose, V.
Altamirano, D.
Jonker, P. G.
van der Klis, M.
Kuiper, L.
Kaiser, C.
Casella, P.
TI A parsec scale X-ray extended structure from the X-ray binary Circinus
X-1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: jets and outflow; stars: individual: Cir X-1; X-rays: binaries
ID RESOLUTION CAMERA HRC; RELATIVISTIC OUTFLOW; CIR X-1; RADIO; JET;
DISCOVERY; STAR; COMPANION; MODEL; AXAF
AB We present the results of the analysis of two Chandra observations of Circinus X-1 performed in 2007, for a total exposure time of similar to 50 ks. The source was observed with the High Resolution Camera during a long X-ray low-flux state of the source. Cir X-1 is an accreting neutron star binary system that exhibits ultra-relativistic arcsec-scale radio jets and an extended arcmin-scale radio nebula. Furthermore, a recent paper has shown an X-ray excess on arcmin-scale prominent on the side of the receding radio jet. In our images, we clearly detect X-ray structures on both the side of the receding and the approaching radio jet. The X-ray emission is consistent with a synchrotron origin. Our detection is consistent with neutron star binaries being as efficient as black hole binaries in producing X-ray outflows, despite their shallower gravitational potential.
C1 [Soleri, P.; Fender, R.; Wijnands, R.; Tudose, V.; Altamirano, D.; van der Klis, M.; Casella, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53705 USA.
[Fender, R.; Kaiser, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Tudose, V.] Acad Romana, Astron Inst, RO-040557 Bucharest, Romania.
[Tudose, V.] Res Ctr Atom Phys & Astrophys, RO-077125 Bucharest, Romania.
[Jonker, P. G.; Kuiper, L.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Soleri, P (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands.
EM p.soleri@uva.nl
RI Tudose, Valeriu/F-8976-2010;
OI Heinz, Sebastian/0000-0002-8433-8652; Casella,
Piergiorgio/0000-0002-0752-3301
FU NWO
FX The authors thank Harvey Tannanbaum for scheduling the DDT observations
and Alessandro Patruno and Dave Russell for very useful comments and
discussion. PS would also like to thank Nanda Rea, Simone Migliari and
the Chandra Help Desk for very useful suggestions on the Chandra data
analysis. PS and PGJ also acknowledge support from NWO.
NR 36
TC 12
Z9 12
U1 0
U2 2
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL 21
PY 2009
VL 397
IS 1
BP L1
EP L5
DI 10.1111/j.1745-3933.2008.00574.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 482XE
UT WOS:000268923100001
ER
PT J
AU Trump, JR
Impey, CD
Kelly, BC
Elvis, M
Merloni, A
Bongiorno, A
Gabor, J
Hao, H
McCarthy, PJ
Huchra, JP
Brusa, M
Cappelluti, N
Koekemoer, A
Nagao, T
Salvato, M
Scoville, NZ
AF Trump, Jonathan R.
Impey, Chris D.
Kelly, Brandon C.
Elvis, Martin
Merloni, Andrea
Bongiorno, Angela
Gabor, Jared
Hao, Heng
McCarthy, Patrick J.
Huchra, John P.
Brusa, Marcella
Cappelluti, Nico
Koekemoer, Anton
Nagao, Tohru
Salvato, Mara
Scoville, Nick Z.
TI OBSERVATIONAL LIMITS ON TYPE 1 ACTIVE GALACTIC NUCLEUS ACCRETION RATE IN
COSMOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; quasars: emission lines; quasars: general
ID BLACK-HOLE MASSES; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY;
WIDE-FIELD SURVEY; LUMINOSITY RELATIONSHIP; EDDINGTON RATIOS; HOST
GALAXIES; REVERBERATION; QUASARS; EMISSION
AB We present black hole masses and accretion rates for 182 Type 1 active galactic nuclei (AGNs) in COSMOS. We estimate masses using the scaling relations for the broad H beta, Mg II, and C IV emission lines in the redshift ranges 0.16 < z < 0.88, 1 < z < 2.4, and 2.7 < z < 4.9. We estimate the accretion rate using an Eddington ratio L(I)/L(Edd) estimated from optical and X-ray data. We find that very few Type 1 AGNs accrete below L(I)/L(Edd) similar to 0.01, despite simulations of synthetic spectra which show that the survey is sensitive to such Type 1 AGNs. At lower accretion rates the broad-line region may become obscured, diluted, or nonexistent. We find evidence that Type 1 AGNs at higher accretion rates have higher optical luminosities, as more of their emission comes from the cool (optical) accretion disk with respect to shorter wavelengths. We measure a larger range in accretion rate than previous works, suggesting that COSMOS is more efficient at finding low accretion rate Type 1 AGNs. However, the measured range in accretion rate is still comparable to the intrinsic scatter from the scaling relations, suggesting that Type 1 AGNs accrete at a narrow range of Eddington ratio, with L(I)/L(Edd) similar to 0.1.
C1 [Trump, Jonathan R.; Impey, Chris D.; Gabor, Jared] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kelly, Brandon C.; Elvis, Martin; Hao, Heng; Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Merloni, Andrea; Bongiorno, Angela; Brusa, Marcella; Cappelluti, Nico] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kelly, Brandon C.; Bongiorno, Angela] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[McCarthy, Patrick J.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
[Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Nagao, Tohru] Ehime Univ, Matsuyama, Ehime 7908577, Japan.
[Salvato, Mara; Scoville, Nick Z.] CALTECH, Pasadena, CA 91125 USA.
RP Trump, JR (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
OI Bongiorno, Angela/0000-0002-0101-6624; Cappelluti,
Nico/0000-0002-1697-186X; Koekemoer, Anton/0000-0002-6610-2048
FU NSF ADP [NNX08AJ28G]; ARCS; NASA through Hubble Fellowship
[HF-01220.01]; Space Telescope Science Institute; Association of
Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]
FX We thank Brad Peterson for helpful discussions on emission line
measurements and Misty Bentz for comments on host contamination. We
thank Marianne Vestergaard for providing the Fe templates and for
discussions on the scaling relations. Amy Stutz and Aleks Diamond-Stanic
provided useful discussions on statistics. J.R.T acknowledges support
from NSF ADP grant NNX08AJ28G and an ARCS fellowship. B. C. K
acknowledges support from NASA through Hubble Fellowship grant
#HF-01220.01 awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS 5-26555.
NR 50
TC 48
Z9 48
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2009
VL 700
IS 1
BP 49
EP 55
DI 10.1088/0004-637X/700/1/49
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 467UP
UT WOS:000267768900004
ER
PT J
AU Krick, JE
Surace, JA
Thompson, D
Ashby, MLN
Hora, JL
Gorjian, V
Yan, L
AF Krick, J. E.
Surace, J. A.
Thompson, D.
Ashby, M. L. N.
Hora, J. L.
Gorjian, V.
Yan, L.
TI GALAXY CLUSTERS IN THE IRAC DARK FIELD. II. MID-INFRARED SOURCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: active; galaxies: clusters: general;
galaxies: evolution; galaxies: photometry; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION HISTORY; HIGH-REDSHIFT CLUSTERS;
PHOTOMETRIC REDSHIFTS; FORMING GALAXIES; LUMINOSITY FUNCTION; STARBURST
GALAXIES; INFRARED GALAXIES; ELLIPTIC GALAXIES; ISOCAM SURVEY
AB We present infrared (IR) luminosities, star formation rates (SFR), colors, morphologies, locations, and active galactic nuclei (AGNs) properties of 24 mu m detected sources in photometrically detected high-redshift clusters in order to understand the impact of environment on star formation (SF) and AGN evolution in cluster galaxies. We use three newly identified z = 1 clusters selected from the IRAC dark field; the deepest ever mid-IR survey with accompanying, 14 band multiwavelength data including deep Hubble Space Telescope imaging and deep wide-area Spitzer MIPS 24 mu m imaging. We find 90 cluster members with MIPS detections within two virial radii of the cluster centers, of which 17 appear to have spectral energy distributions dominated by AGNs and the rest dominated by SF. We find that 43% of the star-forming sample have IR luminosities L-IR > 10(11) L-circle dot (luminous IR galaxies). The majority of sources (81%) are spirals or irregulars. A large fraction (at least 25%) show obvious signs of interactions. The MIPS-detected member galaxies have varied spatial distributions as compared to the MIPS-undetected members with one of the three clusters showing SF galaxies being preferentially located on the cluster outskirts, while the other two clusters show no such trend. Both the AGN fraction and the summed SFR of cluster galaxies increase from redshift zero to one, at a rate that is a few times faster in clusters than over the same redshift range in the field. Cluster environment does have an effect on the evolution of both AGN fraction and SFR from redshift one to the present, but does not affect the IR luminosities or morphologies of the MIPS sample. SF happens in the same way regardless of environment making MIPS sources look the same in the cluster and field, however the cluster environment does encourage a more rapid evolution with time as compared to the field.
C1 [Krick, J. E.; Surace, J. A.; Yan, L.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
[Ashby, M. L. N.; Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Krick, JE (reprint author), CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
EM jkrick@caltech.edu
FU National Aeronautics and Space Administration; National Science
Foundation; NASA [10521, 5-26555]
FX This research has made use of data from the Two Micron All Sky Survey,
which is a joint project of the University of Massachusetts and the
Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This work was based on observations
obtained with the Hale Telescope, Palomar Observatory as part of a
continuing collaboration between the California Institute of Technology,
NASA/JPL, and Cornell University, the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA, the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona,
and the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
observations are associated with program #10521. Support for program
#10521 was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
NR 65
TC 9
Z9 9
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2009
VL 700
IS 1
BP 123
EP 136
DI 10.1088/0004-637X/700/1/123
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 467UP
UT WOS:000267768900011
ER
EF