FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Moran, E Funk, VA AF Moran, Emily Funk, V. A. TI A revision of Erato (Compositae : Liabeae) SO SYSTEMATIC BOTANY LA English DT Article DE Asteraceae; biogeography; Compositae; endemic; phylogeny; taxonomy AB Erato DC. contains five species, distributed from Costa Rica to Bolivia, with its main center of diversity in Ecuador. The revision includes a new species endemic to Costa Rica and Panama, Erato costaricensis E. Moran & V A. Funk. Morphological and molecular data support Erato as a monophyletic group, sister to Philoglossa. The phylogenetic analysis based on morphology used Munnozia Ruiz & Pavon, Chrysactinium (H.B.K.) Wedd., and Philoglossa DC. as outgroups. The phylogeny supports the monophyly of Erato, but the relationships among the species within Erato have only weak support. The genus is believed to be a recent radiation because of the morphological similarity among the taxa and their location in some of the youngest areas of the Andes. C1 Duke Univ, Durham, NC 27708 USA. Smithsonian Inst, US Natl Herbarium, Museum Natl Hist Nat, Washington, DC 20013 USA. RP Moran, E (reprint author), Duke Univ, Durham, NC 27708 USA. EM emily.moran@duke.edu NR 15 TC 2 Z9 2 U1 0 U2 0 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2006 VL 31 IS 3 BP 597 EP 609 PG 13 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 084ZR UT WOS:000240573400015 ER PT J AU Brown, JK AF Brown, Julie K. TI The corporate eye: Photography and the rationalization of American commercial culture. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Brown, JK (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 J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2006 VL 47 IS 3 BP 648 EP 649 DI 10.1353/tech.2006.0164 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 073VO UT WOS:000239770900016 ER PT J AU Wright, HE AF Wright, Helena E. TI Victor Regnault and the advance of photography: The art of avoiding errors. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Wright, HE (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 J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2006 VL 47 IS 3 BP 650 EP 651 DI 10.1353/tech.2006.0211 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 073VO UT WOS:000239770900017 ER PT J AU Warner, DJ AF Warner, Deborah Jean TI Defining women's scientific enterprise: Mount Holyoke Faculty and the rise of American science. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (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 J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2006 VL 47 IS 3 BP 697 EP 698 DI 10.1353/tech.2006.0208 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 073VO UT WOS:000239770900044 ER PT J AU Pope, CE Songsasen, N AF Pope, CE Songsasen, N TI Feline Reproduction: A special issue in honour of professor V.M Shille - Foreword SO THERIOGENOLOGY LA English DT Editorial Material C1 Audubon Nat Inst Res Ctr, New Orleans, LA 70131 USA. Smithsonians Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Pope, CE (reprint author), Audubon Nat Inst Res Ctr, 14001 River Rd, New Orleans, LA 70131 USA. EM epope@auduboninstitute.org; SongsasenN@si.edu NR 0 TC 0 Z9 0 U1 1 U2 3 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JUL 1 PY 2006 VL 66 IS 1 BP 2 EP 2 DI 10.1016/j.theriogenology.2006.04.002 PG 1 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 057WY UT WOS:000238627100001 ER PT J AU Brown, JL AF Brown, JL TI Comparative endocrinology of domestic and nondomestic felids SO THERIOGENOLOGY LA English DT Article DE hormones; fecal steroids; ovary; reproduction; females; felids; stress; hormone ID CHEETAH ACINONYX-JUBATUS; NORMAL ESTROUS-CYCLE; LION PANTHERA-LEO; OVARIAN ACTIVITY; LUTEINIZING-HORMONE; SEXUAL-BEHAVIOR; ADRENOCORTICAL FUNCTION; CHORIONIC-GONADOTROPIN; SERUM CONCENTRATIONS; PLASMA-CONCENTRATIONS AB The ability to track gonadal and adrenal activity via hormones is key to optimizing health and reproduction. Through decades of study, a great deal has been learned about the biology of female domestic cats, including endocrine function. More recently, comparative endocrine studies have greatly expanded our knowledge base of nondomestic felids as well. The latter has been possible largely through the development of noninvasive fecal steroid metabolite analysis techniques, which currently is the method of choice for monitoring endocrine function in wildlife species, including felids. It now is well-recognized that a range in endocrine patterns exists among Felidae, with many traits and mechanisms being uncommon, if not unique. There is a high degree of variability in the type of ovulation (spontaneous versus induced) expressed across the taxon. Even within species, some individuals exhibit ovulation that is only induced, whereas others ovulate spontaneously as well. Steroid metabolism also differs in that metabolites are excreted almost exclusively in feces, with very little steroid found in urine. Across species there are marked differences in seasonal and social influences on reproduction, adrenal responses to husbandry practices, and ovarian responses to assisted reproductive procedures. This means that developing strategies to improve health and reproduction of felids must be done on a species by species basis. This paper summarizes current knowledge on the reproductive endocrinology of female domestic and nondomestic cats, and describes how the rapidly growing endocrine database is aiding ex. situ management efforts. (c) 2006 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM jbrown@si.edu NR 71 TC 63 Z9 67 U1 5 U2 62 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JUL 1 PY 2006 VL 66 IS 1 BP 25 EP 36 DI 10.1016/j.theriogenology.2006.03.011 PG 12 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 057WY UT WOS:000238627100005 PM 16620933 ER PT J AU Pelican, KM Wildt, DE Pukazhenthi, B Howard, J AF Pelican, KM Wildt, DE Pukazhenthi, B Howard, J TI Ovarian control for assisted reproduction in the domestic cat and wild felids SO THERIOGENOLOGY LA English DT Article DE exogenous gonadotropins; ovarian stimulation; follicular inhibition; IVF/Al; felids ID TIGER PANTHERA-TIGRIS; LAPAROSCOPIC ARTIFICIAL-INSEMINATION; GONADOTROPIN-RELEASING-HORMONE; INTRAUTERINE HORN INSEMINATION; HUMAN CHORIONIC-GONADOTROPIN; LEOPARD NEOFELIS-NEBULOSA; CHEETAH ACINONYX-JUBATUS; NON-BREEDING SEASON; IN-VITRO; EXOGENOUS GONADOTROPINS AB Of the 37 felid species, all but the domestic cat are classified as threatened with extinction in all or part of their native range. Additionally, the domestic cat is a valuable model for human biomedical research. Propagating some wild felids as well as domestic cat populations serving as human models is a major challenge primarily due to difficulties in transporting animals between facilities to ensure the pairing of genetically matched individuals, behavioral incompatibility between pairs and low fertility. Artificial insemination (AI) and in vitro fertilization/embryo transfer (IVF/ET) are powerful tools for helping manage rare populations. Developing successful assisted reproductive techniques requires knowledge of the female reproductive cycle and precise control of ovarian activity. Successful ovarian stimulation for AI and IVF/ET has been achieved in at least one-third of all cat species. However, sensitivity to a given gonadotropin treatment appears highly species-specific, and poor responses are common, particularly in felid species that exhibit spontaneous ovulations. Furthermore, current gonadotropin regimens have been demonstrated to perturb female reproductive function often leading to reduced fertility. Overall, ovarian response to exogenous hormonal stimulation has been highly variable, and pregnancy success after AI or IVF/ET remains low (< 20%) in most species. Therefore, there is an immediate need to develop improved regimens that would allow more predictable ovarian responses in felids. We contend that recent research involving the use of progestins to control the ovary prior to gonadotropin stimulation shows promise for providing consistent ovarian stimulation in felids. (c) 2006 Elsevier Inc. All rights reserved. C1 Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Pelican, KM (reprint author), Conservat & Res Ctr, Dept Reprod Sci, Smithsonians Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM kpelican@si.edu FU NCRR NIH HHS [1 K0 01 RR17310-10] NR 98 TC 48 Z9 49 U1 4 U2 36 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JUL 1 PY 2006 VL 66 IS 1 BP 37 EP 48 DI 10.1016/j.theriogenology.2006.03.013 PG 12 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 057WY UT WOS:000238627100006 PM 16630653 ER PT J AU Pukazhenthi, BS Neubauer, K Jewgenow, K Howard, J Wildt, DE AF Pukazhenthi, Budhan S. Neubauer, Katrin Jewgenow, Katarina Howard, JoGayle Wildt, David E. TI The impact and potential etiology of teratospermia in the domestic cat and its wild relatives SO THERIOGENOLOGY LA English DT Article DE testis; spermatogenesis; sperm function ID LIONS PANTHERA-LEO; PHYLOGEOGRAPHIC PATTERNS; EPIDIDYMAL SPERMATOZOA; INVITRO FERTILIZATION; NGORONGORO CRATER; ACROSOME REACTION; GENETIC-VARIATION; SERENGETI PLAINS; SPERM MORPHOLOGY; AMERICAN ZOOS AB Teratospermia (production of > 60% morphologically abnormal sperm/ejaculate) is relatively common among various species in the family Felidae, which is comprised of 37 species. Over two decades of research in this area have produced a significant understanding of the phenotypic expression, its impacts on sperm function and etiology. There is good evidence suggesting that a reduction in genetic diversity contributes to this phenomenon. Results to date demonstrate that spermatozoa from teratospermic donors are compromised in the ability to undergo capacitation and the acrosome reaction, penetrate the zona-pellucida, fertilize conspecific oocytes and survive cryopreservation. Recent studies also reveal abnormalities in chromatin integrity in sperm from teratospermic donors, which, interestingly, fails to impact fertilization or embryo development after intracytoplasmic sperm injection. Through planned inbreeding studies, we now have established that teratospermic cats also produce more spermatozoa by virtue of more sperm producing tissue, more germ cells per Sertoli cell and reduced germ cell loss during spermatogenesis. Overall, it now is clear that gain in sperm quantity is achieved at the expense of sperm quality, suggesting an extensive disruption of normal testicular function in teratospermic donors. Preliminary studies on testicular gene expression in teratospermic cats have also revealed abnormal expression patterns. These findings have markedly increased our understanding of testis biology in the teratospermic donor and reaffirm the value of cats, including wild species, as models for studying novel regulatory mechanisms controlling spermatogenesis and spermiogenesis. Published by Elsevier Inc. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Inst Zoo & Wildlife Res, D-10252 Berlin, Germany. RP Pukazhenthi, BS (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM pukazhenthib@si.edu FU NCRR NIH HHS [K01 RR00135] NR 62 TC 58 Z9 60 U1 2 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD JUL 1 PY 2006 VL 66 IS 1 BP 112 EP 121 DI 10.1016/j.theriogenology.2006.03.020 PG 10 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 057WY UT WOS:000238627100013 PM 16644003 ER PT J AU Theobald, JC Greiner, B Weislo, WT Warrant, EJ AF Theobald, JC Greiner, B Weislo, WT Warrant, EJ TI Visual summation in night-flying sweat bees: A theoretical study SO VISION RESEARCH LA English DT Article DE nocturnal vision; noise; neural summation; apposition compound eyes; halictid bees ID MEGALOPTA-GENALIS; NOCTURNAL BEE; HALICTID BEE; COMPOUND EYE; VISION; LIGHT; DESIGN; ACUITY; PHOTORECEPTORS; TRANSDUCTION AB Bees are predominantly diurnal; only a few groups fly at night. An evolutionary limitation that bees must overcome to inhabit dim environments is their eye type: bees possess apposition compound eyes, which are poorly suited to vision in dim light. Here, we theoretically examine how nocturnal bees Megalopta genalis fly at light levels usually reserved for insects bearing more sensitive superposition eyes. We find that neural summation should greatly increase M. genalis's visual reliability. Predicted spatial summation closely matches the morphology of laminal neurons believed to mediate such summation. Improved reliability costs acuity, but dark adapted bees already suffer optical blurring, and summation further degrades vision only slightly. (c) 2006 Elsevier Ltd. All rights reserved. C1 Lund Univ, Dept Cell & Organism Biol, S-22362 Lund, Sweden. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Theobald, JC (reprint author), Lund Univ, Dept Cell & Organism Biol, Helgonavagen 3, S-22362 Lund, Sweden. EM Jamie.Theobald@cob.lu.se NR 39 TC 38 Z9 39 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0042-6989 J9 VISION RES JI Vision Res. PD JUL PY 2006 VL 46 IS 14 BP 2298 EP 2309 DI 10.1016/j.visres.2006.01.002 PG 12 WC Neurosciences; Ophthalmology SC Neurosciences & Neurology; Ophthalmology GA 058ZK UT WOS:000238702900012 PM 16488460 ER PT J AU Santini, F Tyler, JC Bannikov, AF Baciu, DS AF Santini, F Tyler, JC Bannikov, AF Baciu, DS TI A phylogeny of extant and fossil buckler dory fishes, family Zeidae (Zeiformes, Acanthomorpha) SO CYBIUM LA French DT Article DE Zeiformes; Zeidae; fossils; osteology; phylogeny ID TETRAODONTIFORMES; EVOLUTION AB A data set of 45 putatively informative morphological characters (mostly osteological, and a few external features) is analyzed for 12 extant and fossil species belonging to the buckler dory fish genera Zeus and Zenopsis, which together constitute the family Zeidae (Zeiformes, Acanthomorpha), and for two outgroup taxa. Zeus consists of two extant and three fossil species, whereas Zenopsis consists of four extant and three fossil species. Both genera date back to at least the Oligocene (36 Mya). The phylogenetic analysis of the full data set (extant + fossil) provides strong support for the monophyly of the Zeidae but only weak support for the monophyly of Zenopsis, and it calls into question the existence of a clade formed by the extant and fossil taxa assigned to Zeus. Additional phylogenctic analyses were performed: (1) the most incomplete fossil taxon, Zeus robustus, was excluded; (2) all fossil taxa were excluded; and (3) the new extant species of Zenopsis was excluded. All of these analyses confirm a strongly supported clade formed by Zeus + Zenopsis and of a much less strongly supported clade formed by the extant and fossil species of Zenopsis. The analyses do not provide support for a clade formed by extant and fossil species previously assigned to the genus Zeus, even though when the fossil species are excluded from the analysis, the two extant species of Zeus appear as each other's sister groups in one of three equally parsimonious cladograms. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Russian Acad Sci, Paleontol Inst, Moscow 117997, Russia. Muzeul Stiinte Nat, Piatra Neamt 5600, Romania. Museum Natl Hist Nat, UMR 7138, Dept Syst & Evolut, F-752311 Paris 05, France. RP Santini, F (reprint author), Univ Toronto, Dept Zool, Toronto, ON M5S 3G5, Canada. EM francesco.santini@utoronto.ca; tyler.jim@NMNH.SI.EDU; aban@paleo.ru; dsbaciu@ambra.ro RI Bannikov, Alexander/P-9902-2015 NR 20 TC 3 Z9 3 U1 0 U2 3 PU SOC FRANCAISE D ICHTYOLOGIE PI PARIS PA MUSEUM NATL D HISTOIRE NATURELLE, 43 RUE CUVIER, 75231 PARIS, FRANCE SN 0399-0974 J9 CYBIUM JI Cybium PD JUN 30 PY 2006 VL 30 IS 2 BP 99 EP 107 PG 9 WC Zoology SC Zoology GA 057PE UT WOS:000238606900001 ER PT J AU Thompson, TW Campbell, BA Ghent, RR Hawke, BR Leverington, DW AF Thompson, Thomas W. Campbell, Bruce A. Ghent, Rebecca R. Hawke, B. Ray Leverington, David W. TI Radar probing of planetary regoliths: An example from the northern rim of Imbrium basin SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR; MARS; DEPOSITS; REGION; MOON; WAVELENGTH; IMAGES AB [ 1] Imaging radar measurements at long wavelengths ( e. g., > 30 cm) allow deep ( up to tens of meters) probing of the physical structure and dielectric properties of planetary regoliths. We illustrate a potential application for a Mars orbital synthetic aperture radar ( SAR) using new Earth- based 70-cm wavelength radar data for the Moon. The terrae on the northern margin of Mare Imbrium, the Montes Jura region, have diffuse radar backscatter echoes that are 2 - 4 times weaker at 3.8- cm, 70- cm, and 7.5- m wavelengths than most other lunar nearside terrae. Possible geologic explanations are ( 1) a pyroclastic deposit associated with sinuous rilles in this region, ( 2) buried mare basalt or a zone of mixed highland/ basaltic debris ( cryptomaria), or ( 3) layers of ejecta associated with the Iridum and Plato impacts that have fewer meter-sized rocks than typical highlands regolith. While radar data at 3.8- cm to 7.5- m wavelengths suggest significant differences between the Montes Jura region and typical highlands, the surface geochemistry and rock abundance inferred from Clementine UV-VIS data and eclipse thermal images are consistent with other lunar terrae. There is no evidence for enhanced iron abundance, expected for basaltic pyroclastic deposits, near the source vents of the sinuous rilles radial to Plato. The regions of low 70- cm radar return are consistent with overlapping concentric "haloes'' about Iridum and Plato and do not occur preferentially in topographically low areas, as is observed for radar-mapped cryptomaria. Thus we suggest that the extensive radar-dark area associated with the Montes Jura region is due to overlapping, rock-poor ejecta deposits from Iridum and Plato craters. Comparison of the radial extent of low-radar-return crater haloes with a model for ejecta thickness shows that these rock-poor layers are detected by 70- cm radar where they are on the order of 10 m and thicker. A SAR in orbit about Mars could use similar deep probing to reveal the nature of crater-and basin-related deposits. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Thompson, TW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 300-227, Pasadena, CA 91109 USA. EM thomas.w.thompson@jpl.nasa.gov; campbellb@si.edu; ghentr@si.edu; hawke@higp.hawaii.edu; david.leverington@ttu.edu NR 30 TC 12 Z9 13 U1 0 U2 4 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 JUN 30 PY 2006 VL 111 IS E6 AR E06S14 DI 10.1029/2005JE002566 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 062KE UT WOS:000238942200002 ER PT J AU Smith, JT Jackson, JBC Fortunato, H AF Smith, J. Travis Jackson, Jeremy B. C. Fortunato, Helena TI Diversity and abundance of tropical American scallops (Bivalvia : Pectinidae) from opposite sides of the central American Isthmus SO VELIGER LA English DT Article ID PANAMA LAND-BRIDGE; WESTERN ATLANTIC; MASS EXTINCTION; MARINE BIVALVES; PHYLOGENY; MOLLUSKS; HISTORY; NEOGENE; DIVERGENCE; 16S AB There is confusion about the comparative diversity of mollusks on opposite sides of the Isthmus of Panama due to inadequate sampling and contrasting patterns of diversity for different molluscan taxa. We report here on the occurrence of scallops (Bivalvia: Pectinidae) from extensive new dredge sample collections from the Gulf of Panama and Gulf of Chiriqui in the Eastern Pacific and from the San Blas archipelago to the Cochinos Cays in the Gulf of Honduras in the southwestern Caribbean. The collections contain more than 8000 specimens of 33 species from 213 collections. These include 22 Caribbean species and 11 Eastern Pacific species. However, the average abundance of scallops per collection is much higher in the Eastern Pacific so that the average number of species per collection was similar in the two oceans. This discrepancy in abundance is the principal reason previous workers have erroneously concluded that species diversity is equal or even greater in the Eastern Pacific than the Caribbean. Numbers of scallop species at the seven different Caribbean localities sampled average about one and one half times higher than the two regions in the Eastern Pacific, and the total differences in species richness are two times higher for all the regions combined. Most scallop species were common to abundant and scallop species do not exhibit a log series or log normal pattern of relative abundance. However, we found eight previously undescribed species, two in the Eastern Pacific and six in the Caribbean. These appear to be geminate species and are indistinguishable, pending detailed morphological study, from species occurring in the opposite ocean. These new species are all rare but typically occurred in sufficient abundance and at numerous localities so that their occurrence is not in question. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Ctr Tropical Paleoecol & Archeol, Balboa, Panama. RP Smith, JT (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. NR 71 TC 6 Z9 6 U1 0 U2 2 PU CALIFORNIA MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 USA SN 0042-3211 J9 VELIGER JI Veliger PD JUN 30 PY 2006 VL 48 IS 1 BP 26 EP 45 PG 20 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 060EH UT WOS:000238784700004 ER PT J AU Dorf, M Bosch, H Butz, A Camy-Peyret, C Chipperfield, MP Engel, A Goutail, F Grunow, K Hendrick, F Hrechanyy, S Naujokat, B Pommereau, JP Van Roozendael, M Sioris, C Stroh, F Weidner, F Pfeilsticker, K AF Dorf, M. Boesch, H. Butz, A. Camy-Peyret, C. Chipperfield, M. P. Engel, A. Goutail, F. Grunow, K. Hendrick, F. Hrechanyy, S. Naujokat, B. Pommereau, J. -P. Van Roozendael, M. Sioris, C. Stroh, F. Weidner, F. Pfeilsticker, K. TI Balloon-borne stratospheric BrO measurements: comparison with Envisat/SCIAMACHY BrO limb profiles SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ABSORPTION CROSS-SECTIONS; SOLAR ZENITH ANGLES; DIFFERENT LATITUDES; BROMINE; NO2; OZONE; MODEL; SPECTROSCOPY; SCIAMACHY; SATELLITE AB For the first time, results of four stratospheric BrO profiling instruments, are presented and compared with reference to the SLIMCAT 3-dimensional chemical transport model (3-D CTM). Model calculations are used to infer a BrO profile validation set, measured by 3 different balloon sensors, for the new Envisat/SCIAMACHY (ENVIronment SATellite/SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY) satellite instrument. The balloon observations include ( a) balloon-borne in situ resonance fluorescence detection of BrO ( Triple), (b) balloon-borne solar occultation DOAS measurements ( Differential Optical Absorption Spectroscopy) of BrO in the UV, and ( c) BrO profiling from the solar occultation SAOZ ( Systeme d'Analyse par Observation Zenithale) balloon instrument. Since stratospheric BrO is subject to considerable diurnal variation and none of the measurements are performed close enough in time and space for a direct comparison, all balloon observations are considered with reference to outputs from the 3-D CTM. The referencing is performed by forward and backward air mass trajectory calculations to match the balloon with the satellite observations. The diurnal variation of BrO is considered by 1-D photochemical model calculation along the trajectories. The 1-D photochemical model is initialised with output data of the 3-D model with additional constraints on the vertical transport, the total amount and photochemistry of stratospheric bromine as given by the various balloon observations. Total [Br(y)]=(20.1 +/- 2.5) pptv obtained from DOAS BrO observations at mid-latitudes in 2003, serves as an upper limit of the comparison. Most of the balloon observations agree with the photochemical model predictions within their given error estimates. First retrieval exercises of BrO limb profiling from the SCIAMACHY satellite instrument on average agree to around 20% with the photochemically-corrected balloon observations of the remote sensing instruments (SAOZ and DOAS). An exception is the in situ Triple profile, in which the balloon and satellite data mostly does not agree within the given errors. In general, the satellite measurements show systematically higher values below 25 km than the balloon data and a change in profile shape above about 25 km. C1 Univ Heidelberg, Inst Umweltphys, D-6900 Heidelberg, Germany. Univ Paris 06, LPMAA, Paris, France. Univ Leeds, Sch Earth & Environm, Inst Atmospher Sci, Leeds, W Yorkshire, England. Goethe Univ Frankfurt, Inst Atmosphere & Environm, D-6000 Frankfurt, Germany. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Free Univ Berlin, Inst Meteorol, D-1000 Berlin, Germany. Belgian Inst Space Aeron, BIRA, IASB, Brussels, Belgium. Forschungszentrum Julich, Inst Chem & Dynam Geosphare ICG Stratosphare 1, Julich, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dorf, M (reprint author), Univ Heidelberg, Inst Umweltphys, D-6900 Heidelberg, Germany. EM marcel.dorf@iup.uni-heidelberg.de RI Stroh, Fred/A-6505-2009; Butz, Andre/A-7024-2013; Chipperfield, Martyn/H-6359-2013; Boesch, Hartmut/G-6021-2012; Engel, Andreas/E-3100-2014; OI Stroh, Fred/0000-0002-4492-2977; Butz, Andre/0000-0003-0593-1608; Chipperfield, Martyn/0000-0002-6803-4149; Engel, Andreas/0000-0003-0557-3935; Sioris, Christopher/0000-0003-1168-8755 NR 54 TC 35 Z9 35 U1 1 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD JUN 29 PY 2006 VL 6 BP 2483 EP 2501 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 058OZ UT WOS:000238675600010 ER PT J AU Kornicker, LS Van Bakel, BWM Fraaije, RHB Jagt, JWM AF Kornicker, Louis S. Van Bakel, Barry W. M. Fraaije, Rene H. B. Jagt, John W. M. TI Revision of Mesozoic Myodocopina (Ostracoda) and a new genus and species, Mesoleberis hollandica, from the Upper Cretaceous of Belgium and The Netherlands SO ZOOTAXA LA English DT Review DE Ostracoda; Myodocopida; Mesozoic; Cretaceous; The Netherlands; Belgium; new genus; new species ID CRABS CRUSTACEA; DECAPODA; BRACHYURA AB Although Paleozoic strata have produced many ostracode fossils in the suborder Myodocopina, which are also abundant in today's seas, their record is extremely sparse in Mesozoic strata. A new genus and species of myodocopid, Mesoleberis hollandica, from the upper Maastrichtian ( Upper Cretaceous) of the southeast Netherlands and nearby Belgium is described herein. In addition, brief supplementary descriptions and illustrations are presented of other Myodocopina that have been reported from Mesozoic deposits; many of those species are referred to different genera, and six are placed in the category "species nomina dubia." C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Oertijdmuseum Groene Poort, NL-5283 WB Boxtel, Netherlands. Nat Hist Museum Maastricht, NL-6211 KJ Maastricht, Netherlands. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM kornickl@si.edu; barry.van.bakel@wolmail.nl; info@oertijdmuseum.nl; john.jagt@maastricht.nl NR 118 TC 3 Z9 3 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 JUN 29 PY 2006 IS 1246 BP 15 EP 54 PG 40 WC Zoology SC Zoology GA 066WV UT WOS:000239262100002 ER PT J AU Davis, JL Wernicke, BP Bisnath, S Niemi, NA Elosegui, P AF Davis, J. L. Wernicke, B. P. Bisnath, S. Niemi, N. A. Elosegui, P. TI Subcontinental-scale crustal velocity changes along the Pacific-North America plate boundary SO NATURE LA English DT Article ID WESTERN UNITED-STATES; NEVADA SEISMIC BELT; CALIFORNIA; EARTHQUAKE; RELAXATION; POSITIONS; VISCOSITY; LANDERS; BENEATH; FAULT AB Transient tectonic deformation has long been noted within similar to 100 km of plate boundary fault zones and within active volcanic regions, but it is unknown whether transient motions also occur at larger scales within plates. Relatively localized transients are known to occur as both seismic and episodic aseismic events(1), and are generally ascribed to motions of magma bodies, aseismic creep on faults, or elastic or viscoelastic effects associated with earthquakes. However, triggering phenomena(2,3) and systematic patterns of seismic strain release at subcontinental (similar to 1,000 km) scale along diffuse plate boundaries(4,5) have long suggested that energy transfer occurs at larger scale. Such transfer appears to occur by the interaction of stresses induced by surface wave propagation and magma or groundwater in the crust(6), or from large-scale stress diffusion within the oceanic mantle in the decades following clusters of great earthquakes(7). Here we report geodetic evidence for a coherent, subcontinental-scale change in tectonic velocity along a diffuse similar to 1,000-km-wide deformation zone. Our observations are derived from continuous GPS (Global Positioning System) data collected over the past decade across the Basin and Range province, which absorbs approximately 25 per cent of Pacific-North America relative plate motion. The observed changes in site velocity define a sharp boundary near the centre of the province oriented roughly parallel to the north-northwest relative plate motion vector. We show that sites to the west of this boundary slowed relative to sites east of it by similar to 1mm yr(-1) starting in late 1999. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Davis, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdavis@cfa.harvard.edu RI Niemi, Nathan/A-9996-2011; Davis, James/D-8766-2013; OI Davis, James/0000-0003-3057-477X; Niemi, Nathan/0000-0002-3380-3024 NR 21 TC 21 Z9 22 U1 2 U2 16 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 JUN 28 PY 2006 VL 441 IS 7097 BP 1131 EP 1134 DI 10.1038/nature04781 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 057SM UT WOS:000238615500046 PM 16810252 ER PT J AU Palmer, PI Abbot, DS Fu, TM Jacob, DJ Chance, K Kurosu, TP Guenther, A Wiedinmyer, C Stanton, JC Pilling, MJ Pressley, SN Lamb, B Sumner, AL AF Palmer, Paul I. Abbot, Dorian S. Fu, Tzung-May Jacob, Daniel J. Chance, Kelly Kurosu, Thomas P. Guenther, Alex Wiedinmyer, Christine Stanton, Jenny C. Pilling, Michael J. Pressley, Shelley N. Lamb, Brian Sumner, Anne Louise TI Quantifying the seasonal and interannual variability of North American isoprene emissions using satellite observations of the formaldehyde column SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID VOLATILE ORGANIC-COMPOUNDS; OZONE MONITORING EXPERIMENT; MASTER CHEMICAL MECHANISM; MCM V3 PART; TROPOSPHERIC DEGRADATION; SURFACE REFLECTIVITY; MODEL DESCRIPTION; GOCART MODEL; GLOBAL-MODEL; ART. AB [ 1] Quantifying isoprene emissions using satellite observations of the formaldehyde ( HCHO) columns is subject to errors involving the column retrieval and the assumed relationship between HCHO columns and isoprene emissions, taken here from the GEOSCHEM chemical transport model. Here we use a 6-year ( 1996 - 2001) HCHO column data set from the Global Ozone Monitoring Experiment (GOME) satellite instrument to ( 1) quantify these errors, ( 2) evaluate GOME-derived isoprene emissions with in situ flux measurements and a process-based emission inventory ( Model of Emissions of Gases and Aerosols from Nature, MEGAN), and ( 3) investigate the factors driving the seasonal and interannual variability of North American isoprene emissions. The error in the GOME HCHO column retrieval is estimated to be 40%. We use the Master Chemical Mechanism (MCM) to quantify the time-dependent HCHO production from isoprene, alpha-and beta-pinenes, and methylbutenol and show that only emissions of isoprene are detectable by GOME. The time-dependent HCHO yield from isoprene oxidation calculated by MCM is 20 - 30% larger than in GEOS-CHEM. GOME-derived isoprene fluxes track the observed seasonal variation of in situ measurements at a Michigan forest site with a - 30% bias. The seasonal variation of North American isoprene emissions during 2001 inferred from GOME is similar to MEGAN, with GOME emissions typically 25% higher ( lower) at the beginning ( end) of the growing season. GOME and MEGAN both show a maximum over the southeastern United States, but they differ in the precise location. The observed interannual variability of this maximum is 20 - 30%, depending on month. The MEGAN isoprene emission dependence on surface air temperature explains 75% of the month-to-month variability in GOME-derived isoprene emissions over the southeastern United States during May - September 1996 - 2001. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Boulder, CO 80303 USA. Univ Leeds, Dept Chem, Leeds LS2 9JT, W Yorkshire, England. Washington State Univ, Dept Civil & Environm Engn, Pullman, WA 99164 USA. Battelle Mem Inst, Columbus, OH 43201 USA. RP Palmer, PI (reprint author), Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. EM pip@env.leeds.ac.uk RI Palmer, Paul/F-7008-2010; Abbot, Dorian/J-6352-2012; Pfister, Gabriele/A-9349-2008; Guenther, Alex/B-1617-2008; Chem, GEOS/C-5595-2014; Fu, Tzung-May/N-3418-2015; OI Guenther, Alex/0000-0001-6283-8288; Chance, Kelly/0000-0002-7339-7577 NR 41 TC 112 Z9 113 U1 3 U2 34 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2006 VL 111 IS D12 AR D12315 DI 10.1029/2005JD006689 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 062IR UT WOS:000238938300005 ER PT J AU Cisneros-Heredia, DF Mcdiarmid, RW AF Cisneros-Heredia, Diego F. Mcdiarmid, Roy W. TI A new species of the genus Centrolene (Amphibia : Anura : Centrolenidae) from Ecuador with comments on the taxonomy and biogeography of Glassfrogs SO ZOOTAXA LA English DT Article DE Centrolene mariaelenae, new species; taxonomy; biogeography; Ecuador ID FROG ANURA; HYALINOBATRACHIUM; PHYLOGENY; VENEZUELA; HYLIDAE; PERU AB We describe a new species of Glassfrog, Centrolene mariaelenae n. sp., from the Contrafuerte de Tzunantza, southeastern Ecuador. The new species is assigned to the Centrolene gorzulai species group, a clade previously known only from the Guayana Shield region, because the parietal peritoneum is transparent and the hepatic peritoneum is covered by guanophores. We analyze the diversity patterns of Glassfrogs from eastern Ecuador. The distribution of the new species herein described supports previous hypothesis of a biogeographical connection between the Andes and the Guayana Shield for various groups of plants and animals; particularly a relationship between the Guayana Shield and the sandstone outcrops mountain ranges of southeastern Ecuador and northeastern Peru. We also comment on the infrageneric and generic classification of Glassfrogs, and propose the new combinations Centrolene balionotum n. comb., Cochranella antisthenesi n. comb., and Cochranella pulverata n. comb. C1 Smithsonian Inst, Natl Museum Nat Hist, Res Training Program 2002, Washington, DC 20560 USA. Univ San Francisco Quito, Coll Biol & Environm Sci, Quito, Ecuador. US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Cisneros-Heredia, DF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Res Training Program 2002, Washington, DC 20560 USA. EM diegofrancisco_cisneros@yahoo.com; mcdiarmr@nmnh.si.edu RI Cisneros-Heredia, Diego/D-1744-2011 OI Cisneros-Heredia, Diego/0000-0002-6132-2738 NR 70 TC 16 Z9 21 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 26 PY 2006 IS 1244 BP 1 EP 32 PG 32 WC Zoology SC Zoology GA 066WR UT WOS:000239261700001 ER PT J AU Kruckert, K Flachsbarth, B Schulz, S Hentschel, U Weldon, PJ AF Krueckert, Karsten Flachsbarth, Birte Schulz, Stefan Hentschel, Ute Weldon, Paul J. TI Ethyl-branched aldehydes, ketones, and diketones from caimans (Caiman and Paleosuchus; crocodylia, reptilia) SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID DIANEACKERONE; CROCODILE; CHEMISTRY; ESTERS AB Secretions from the paracloacal glands of alligators (Alligator spp.) and caimans (Caiman spp., Melanosuchus niger, and Paleosuchus spp.) were examined by GC-MS. The secretions of the common caiman (C. crocodilus), the broadsnouted caiman (C. latirostris), the yacare caiman (C. yacare), the dwarf caiman (P. palpebrosus), and the smooth-fronted caiman (P. trigonatus) yielded a new family of 43 aliphatic carbonyl compounds that includes aldehydes, ketones, and beta-diketones with an ethyl branch adjacent to the carbonyl group. The identification of these glandular components and the syntheses and stereochemical investigations of selected compounds are described. C1 Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, D-38106 Braunschweig, Germany. Univ Wurzburg, Zentrum Infek Forsch, D-97070 Wurzburg, Germany. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Schulz, S (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, Hagenring 30, D-38106 Braunschweig, Germany. EM stefan.schulz@tu-bs.de RI Hentschel, Ute/H-8343-2013 OI Hentschel, Ute/0000-0003-0596-790X NR 21 TC 8 Z9 9 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD JUN 23 PY 2006 VL 69 IS 6 BP 863 EP 870 DI 10.1021/np0600797 PG 8 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 055VN UT WOS:000238478800001 PM 16792401 ER PT J AU Lotze, HK Lenihan, HS Bourque, BJ Bradbury, RH Cooke, RG Kay, MC Kidwell, SM Kirby, MX Peterson, CH Jackson, JBC AF Lotze, HK Lenihan, HS Bourque, BJ Bradbury, RH Cooke, RG Kay, MC Kidwell, SM Kirby, MX Peterson, CH Jackson, JBC TI Depletion, degradation, and recovery potential of estuaries and coastal seas SO SCIENCE LA English DT Article ID MARINE; ECOSYSTEMS; EXTINCTIONS; RESILIENCE; IMPACTS; FUTURE; OCEANS; FAUNA AB Estuarine and coastal transformation is as old as civilization yet has dramatically accelerated over the past 150 to 300 years. Reconstructed time lines, causes, and consequences of change in 12 once diverse and productive estuaries and coastal seas worldwide show similar patterns: Human impacts have depleted >90% of formerly important species, destroyed >65% of seagrass and wetland habitat, degraded water quality, and accelerated species invasions. Twentieth-century conservation efforts achieved partial recovery of upper trophic levels but have so far failed to restore former ecosystem structure and function. Our results provide detailed historical baselines and quantitative targets for ecosystem-based management and marine conservation. C1 Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. Bates Coll, Dept Anthropol, Lewiston, ME 04240 USA. Australian Natl Univ, Res Sch Pacific & Asian Studie, Resources Management Asia Pacific Program, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Unit 0948, APO, AA 34002 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. RP Lotze, HK (reprint author), Dalhousie Univ, Dept Biol, 1355 Oxford St, Halifax, NS B3H 4J1, Canada. EM hlotze@dal.ca NR 27 TC 1022 Z9 1056 U1 98 U2 689 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 JUN 23 PY 2006 VL 312 IS 5781 BP 1806 EP 1809 DI 10.1126/science.1128035 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 055LS UT WOS:000238452800061 PM 16794081 ER PT J AU Stapley, J Whiting, MJ AF Stapley, Jessica Whiting, Martin J. TI Ultraviolet signals fighting ability in a lizard SO BIOLOGY LETTERS LA English DT Article DE male-male competition; Platysaurus broadleyi; status signal; ultraviolet; communication; sexual selection ID MATE CHOICE; COMPETITION; FLYCATCHER; BEHAVIOR; SIZE; FISH AB Ultraviolet (UV) signals are used in female mate choice in numerous taxa; however, the role of UV signals in male contests remains relatively unexplored. We experimentally reduced throat UV of free-ranging lizards (Platysaurus broadleyi) to test whether UV acts as a signal of fighting ability during male contests. We found that UV-reduced males were more likely to be challenged than control males. However, contest outcome was not influenced by UV-reduction, and this was despite other obvious asymmetries between opponents, such as body size and residency. Throat UV was confirmed as a signal of fighting ability because contests were more likely to escalate when one contestant had reduced UV. Therefore, throat UV, not body size or residency, was used during the initial stage of opponent assessment, but this did not influence contest outcome. The results suggest that UV overrides other traits that could function as signals during rival assessment. C1 Smithsonian Trop Res Inst, Unit 4098, APO AA, Miami, FL 34002 USA. Univ Witwatersrand, Sch Anim Plant & Environm Sci, ZA-2000 Johannesburg, South Africa. RP Stapley, J (reprint author), Smithsonian Trop Res Inst, Unit 4098, APO AA, Miami, FL 34002 USA. EM stapleyi@si.edu RI Stapley, Jessica/B-3858-2010; Whiting, Martin/E-2999-2010; OI Whiting, Martin/0000-0002-4662-0227; Stapley, Jessica/0000-0002-9138-5684 NR 20 TC 48 Z9 50 U1 12 U2 21 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETT-UK JI Biol. Lett. PD JUN 22 PY 2006 VL 2 IS 2 BP 169 EP 172 DI 10.1098/rsbl.2005.0419 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 103CE UT WOS:000241862500003 PM 17148355 ER PT J AU Fallon, SM Fleischer, RC Graves, GR AF Fallon, Sylvia M. Fleischer, Robert C. Graves, Gary R. TI Malarial parasites as geographical markers in migratory birds? SO BIOLOGY LETTERS LA English DT Article DE Dendroica caerulescens; Haemoproteus; Plasmodium; geographical markers; migratory songbirds; parasites ID WARBLERS DENDROICA-CAERULESCENS; AVIAN MALARIA; BLOOD PARASITES; LESSER ANTILLES; STABLE-ISOTOPES; CYTOCHROME-B; CONNECTIVITY; SEQUENCES; SONGBIRD AB We tested the hypothesis that malarial parasites (Plasmodium and Haemoproteus) of black-throated blue warblers (Dendroica caerulescens) provide sufficient geographical signal to track population movements between the warbler's breeding and wintering habitats in North America. Our results from 1083 warblers sampled across the species' breeding range indicate that parasite lineages are geographically widespread and do not provide site-specific information. The wide distribution of malarial parasites probably reflects postnatal dispersal of their hosts as well as mixing of breeding populations on the wintering range. When compared to geographically structured parasites of sedentary Caribbean songbirds, patterns of malarial infections in black-throated blue warblers suggest that host-malaria dynamics of migratory and sedentary bird populations may be subject to contrasting selection pressures. C1 Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Fallon, SM (reprint author), Smithsonian Inst, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM fallons@si.edu FU NIGMS NIH HHS [GM63258-02, R01 GM063258] NR 32 TC 25 Z9 25 U1 2 U2 10 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD JUN 22 PY 2006 VL 2 IS 2 BP 213 EP 216 DI 10.1098/rsbl.2005.0429 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 103CE UT WOS:000241862500014 PM 17148365 ER PT J AU Jamieson, MJ Dalgarno, A Wei, L AF Jamieson, MJ Dalgarno, A Wei, L TI Elastic scattering of hydrogen and deuterium atoms by oxygen atoms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID COLLISION CROSS-SECTIONS; OH; STATES; VENUS AB [ 1] Interaction potentials of Yarkony ( 1992), matched to new dispersion potentials, are used in calculations by quantal and semiclassical methods of scattering and diffusion cross sections for elastic collisions between hydrogen and deuterium atoms and oxygen atoms, at energies up to 5 eV. Discrepancies among the published values and with the new results are resolved. The coefficients that describe mutual diffusion between hydrogen and oxygen and between deuterium and oxygen at temperatures up to 5000 K are calculated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jamieson, MJ (reprint author), Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. EM mjj@dcs.gla.ac.uk; adalgarno@cfa.harvard.edu NR 15 TC 3 Z9 3 U1 1 U2 5 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 JUN 22 PY 2006 VL 111 IS A6 AR A06308 DI 10.1029/2005JA011361 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 057NT UT WOS:000238603200003 ER PT J AU Miller, JM Raymond, J Fabian, A Steeghs, D Homan, J Reynolds, C van der Klis, M Wijnands, R AF Miller, JM Raymond, J Fabian, A Steeghs, D Homan, J Reynolds, C van der Klis, M Wijnands, R TI The magnetic nature of disk accretion onto black holes SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEI; GRO J1655-40; WINDS; DRIVEN; JETS; MASS; SPECTROSCOPY; SIMULATIONS; INSTABILITY; DYNAMICS AB Although disk accretion onto compact objects - white dwarfs, neutron stars and black holes - is central to much of high-energy astrophysics, the mechanisms that enable this process have remained observationally difficult to determine. Accretion disks must transfer angular momentum in order for matter to travel radially inward onto the compact object(1). Internal viscosity from magnetic processes(1-4) and disk winds(5) can both in principle transfer angular momentum, but hitherto we lacked evidence that either occurs. Here we report that an X-ray-absorbing wind discovered in an observation of the stellar-mass black hole binary GRO J1655-40 ( ref. 6) must be powered by a magnetic process that can also drive accretion through the disk. Detailed spectral analysis and modelling of the wind shows that it can only be powered by pressure generated by magnetic viscosity internal to the disk or magnetocentrifugal forces. This result demonstrates that disk accretion onto black holes is a fundamentally magnetic process. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 28 TC 137 Z9 139 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 22 PY 2006 VL 441 IS 7096 BP 953 EP 955 DI 10.1038/nature04912 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 055AT UT WOS:000238422300035 PM 16791188 ER PT J AU Witham, AR Knigge, C Gansicke, BT Aungwerojwit, A Corradi, RLM Drew, JE Greimel, R Groot, PJ Morales-Rueda, L Rodriguez-Flores, ER Rodriguez-Gil, P Steeghs, D AF Witham, AR Knigge, C Gansicke, BT Aungwerojwit, A Corradi, RLM Drew, JE Greimel, R Groot, PJ Morales-Rueda, L Rodriguez-Flores, ER Rodriguez-Gil, P Steeghs, D TI The properties of cataclysmic variables in photometric H alpha surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; binaries : close; novae, cataclysmic variables ID X-RAY BINARIES; EMISSION-LINES; EVOLUTION; POPULATION; EDITION; CATALOG; POLARS; ATLAS; DWARF; MODEL AB We report on the properties of 71 known cataclysmic variables (CVs) in photometric H alpha emission-line surveys. Our study is motivated by the fact that the Isaac Newton Telescope (INT) Photometric H alpha Survey of the northern galactic plane (IPHAS) will soon provide r', i' and narrow-band H alpha measurements down to r' similar or equal to 20 for all northern objects between - 5 degrees < b < +5 degrees. IPHAS thus provides a unique resource, both for studying the emission-line properties of known CVs and for constructing a new CV sample selected solely on the basis of H alpha excess. Our goal here is to carry out the first task and prepare the way for the second. In order to achieve this, we analyse data on 19 CVs already contained in the IPHAS data base and supplement this with identical observations of 52 CVs outside the galactic plane. Our key results are as follows: (i) the recovery rate of known CVs as H alpha emitters in a survey like IPHAS is similar or equal to 70 per cent; (ii) of the similar or equal to 30 per cent of CVs which were not recovered similar or equal to 75 per cent were clearly detected but did not exhibit a significant H alpha excess at the time of our observations; (iii) the recovery rate depends only weakly on CV type; (iv) the recovery rate depends only weakly on orbital period; (v) short-period dwarf novae tend to have the strongest H alpha lines. These results imply that photometric emission-line searches provide an efficient way of constructing CV samples that are not biased against detection of intrinsically faint, short-period systems. C1 Univ Southampton, Sch Phys & Astron, Highfield SO17 1BJ, England. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. Inst Astrofis Canarias, Tenerife 38200, Spain. Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. Radboud Univ Nijmegen, Afdeling Sterrenkunde, Fac NWI, NL-6500 GL Nijmegen, Netherlands. Inst Astron & Geofis, Havana 11600, Cuba. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Witham, AR (reprint author), Univ Southampton, Sch Phys & Astron, Highfield SO17 1BJ, England. EM arw@phys.soton.ac.uk RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016; Rodriguez-Gil, Pablo/H-7709-2015 OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Rodriguez-Gil, Pablo/0000-0002-4717-5102 NR 22 TC 22 Z9 23 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2006 VL 369 IS 2 BP 581 EP 597 DI 10.1111/j.1365-2966.2006.10395.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 050QW UT WOS:000238104000004 ER PT J AU Protopapas, P Giammarco, JM Faccioli, L Struble, MF Dave, R Alcock, C AF Protopapas, P Giammarco, JM Faccioli, L Struble, MF Dave, R Alcock, C TI Finding outlier light curves in catalogues of periodic variable stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; astronomical data bases : miscellaneous; catalogues; binaries : eclipsing; Cepheids; stars : variables : other ID LARGE-MAGELLANIC-CLOUD; GRAVITATIONAL LENSING EXPERIMENT; ECCENTRIC ECLIPSING BINARIES; MASSIVE VARIABILITY SURVEYS; DIFFERENCE IMAGE-ANALYSIS; SKY AUTOMATED SURVEY; RR-LYRAE STARS; MACHO PROJECT; APSIDAL MOTION; SMC DATA AB We present a methodology to discover outliers in catalogues of periodic light curves. We use a cross-correlation as the measure of 'similarity' between two individual light curves, and then classify light curves with lowest average 'similarity' as outliers. We performed the analysis on catalogues of periodic variable stars of known type from the MACHO and OGLE projects. This analysis was carried out in Fourier space and we established that our method correctly identifies light curves that do not belong to those catalogues as outliers. We show how an approximation to this method, carried out in real space, can scale to large data sets that will be available in the near future such as those anticipated from the Panoramic Survey Telescope & Rapid Response System (Pan-STARRS) and Large Synoptic Survey Telescope (LSST). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Protopapas, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pprotopapas@cfa.harvard.edu NR 43 TC 30 Z9 30 U1 0 U2 4 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2006 VL 369 IS 2 BP 677 EP 696 DI 10.1111/j.1365-2966.2006.10327.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 050QW UT WOS:000238104000012 ER PT J AU Green, PJ AF Green, Paul J. TI Lens-aided multi-angle spectroscopy (LAMAS) reveals small-scale outflow structure in quasars SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : absorption lines; quasars : individual (SDSS J1004+4112) ID BROAD-ABSORPTION-LINE; ACTIVE GALACTIC NUCLEI; X-RAY OBSERVATIONS; DIGITAL-SKY-SURVEY; KECK HIRES OBSERVATIONS; EMISSION-LINE; PHYSICAL CONDITIONS; STELLAR OBJECTS; BAL QUASAR; SIMULTANEOUS ULTRAVIOLET AB Spectral differences between lensed quasar image components are common. Since lensing is intrinsically achromatic, these differences are typically explained as the effect of either microlensing, or as light path time delays sampling intrinsic quasar spectral variability. Here we advance a novel third hypothesis: some spectral differences are due to small line-of-sight differences through quasar disk wind outflows. In particular, we propose that variable spectral differences seen only in component A of the widest separation lens SDSS J1004+4112 are due to differential absorption along the sight lines. The absorber properties required by this hypothesis are akin to known broad absorption line (BAL) outflows but must have a broader, smoother velocity profile. We interpret the observed C IV emission-line variability as further evidence for spatial fine structure transverse to the line of sight. Since outflows are likely to be rotating, such absorber fine structure can consistently explain some of the UV and X-ray variability seen in AGNs. The implications are many: (1) Spectroscopic differences in other lensed objects may be due to this ``lens-aided multi-angle spectroscopy'' (LAMAS). (2) Outflows have fine structure on size scales of arcseconds, as seen from the nucleus. (3) Assuming either broad absorption line region sizes proposed in recent wind models, or typically assumed continuum emission region sizes, LAMAS and/or variability provide broadly consistent absorber size scale estimates of similar to 10(15) cm. (4) Very broad smooth absorption may be ubiquitous in quasar spectra, even when no obvious troughs are seen. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu NR 85 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 733 EP 741 DI 10.1086/503760 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100008 ER PT J AU Gutierrez, K Badran, HM Bradbury, SM Buckley, JH Celik, O Chow, YC Cogan, P Cui, W Daniel, M Falcone, A Fegan, SJ Finley, JP Gillanders, GH Grube, J Holder, J Horan, D Hughes, SB Jung, I Kieda, D Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Maier, G Moriarty, P Perkins, J Pohl, M Quinn, J Rebillot, PF Rose, HJ Schroedter, M Sembroski, GH Wakely, SP Weekes, TC White, RJ AF Gutierrez, K Badran, HM Bradbury, SM Buckley, JH Celik, O Chow, YC Cogan, P Cui, W Daniel, M Falcone, A Fegan, SJ Finley, JP Gillanders, GH Grube, J Holder, J Horan, D Hughes, SB Jung, I Kieda, D Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Maier, G Moriarty, P Perkins, J Pohl, M Quinn, J Rebillot, PF Rose, HJ Schroedter, M Sembroski, GH Wakely, SP Weekes, TC White, RJ CA VERITAS Collabor TI Multiwavelength observations of 1ES 1959+650, 1 year after the strong outburst of 2002 SO ASTROPHYSICAL JOURNAL LA English DT Article ID TEV GAMMA-RAYS; BLAZAR 1ES-1959+650; STRONG FLARES; 4.85 GHZ; MKN 501; VARIABILITY; TELESCOPE; RADIATION; EVOLUTION; SPECTRUM AB In 2003 April-May, the blazar 1ES 1959+650 showed an increased level of X-ray activity. This prompted a multiwavelength observation campaign with the Whipple 10 m gamma-ray telescope, the Rossi X-Ray Timing Explorer, the Bordeaux Optical Observatory, and the University of Michigan Radio Astronomy Observatory. We present the multiwavelength data taken from 2003 May 2 to June 7 and compare the source characteristics with those measured during observations taken during the years 2000 and 2002. The X-ray observations gave a data set with high signal-to-noise ratio light curves and energy spectra; however, the gamma-ray observations did not reveal a major TeV gamma-ray flare. Furthermore, we find that the radio and optical fluxes do not show statistically significant deviations from those measured during the 2002 flaring periods. While the X-ray flux and X-ray photon index appear correlated during subsequent observations, the apparent correlation evolved significantly among the years 2000, 2002, and 2003. We discuss the implications of this finding for the mechanism that causes the flaring activity. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Natl Univ Ireland, Dept Phys, Galway, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Observ Bordeaux, OASU, CNRS, UMR 5804, F-33270 Floirac, France. RP Gutierrez, K (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. RI Daniel, Michael/A-2903-2010 OI Daniel, Michael/0000-0002-8053-7910 NR 24 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 742 EP 747 DI 10.1086/503738 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100009 ER PT J AU Dye, S Eales, SA Ashby, MLN Huang, JS Webb, TMA Barmby, P Lilly, S Brodwin, M McCracken, H Egami, E Fazio, GG AF Dye, S. Eales, S. A. Ashby, M. L. N. Huang, J. -S. Webb, T. M. A. Barmby, P. Lilly, S. Brodwin, M. McCracken, H. Egami, E. Fazio, G. G. TI An investigation of the submillimeter background radiation using SCUBA and Spitzer SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; infrared : galaxies; submillimeter ID HUBBLE-DEEP-FIELD; 14 HOUR FIELD; FRANCE REDSHIFT SURVEY; LYMAN BREAK GALAXIES; ARRAY CAMERA IRAC; SPACE-TELESCOPE; SOURCE IDENTIFICATIONS; STARBURST GALAXIES; SCUBA-8-MJY SURVEY; 3-HOUR FIELD AB We investigate the redshift dependence of the contribution to the extragalactic far-infrared/submillimeter background from galaxies detected by the Spitzer Space Telescope at 8 and 24 mu m. Using seven-band optical to mid-infrared photometry, we estimate photometric redshifts for the Spitzer sources that appear to be mostly L-* galaxies at a median redshift of z = 1.0. These sources, extracted from deep 8 and 24 mu m mosaics of the CUDSS 14 hour field with 5 sigma limits of 5.8 and 70 mu Jy, respectively, exhibit significant 850 and 450 mu m emission as observed by SCUBA. At 850 mu m, after removing >= 4 sigma sources and those securely identified in our companion cross-matching paper, we measure stacked flux at the significance level of 4.4 and 2.9 sigma from the full 8 and 24 mu m galaxy catalog, respectively. At 450 mu m, flux is detected from all 8 mu m galaxies at the level of 3.5 sigma, while there is no significant emission from the 24 mu m galaxies. We find that the 850 mu m flux is emitted almost exclusively at z greater than or similar to 1.3 from the Spitzer sources with 0.44 mJy (4.7 sigma) per 8 mu m source, and 0.51 mJy (2.8 sigma) per 24 mu m source. This corresponds to a contribution of (16 +/- 3)% toward the 850 mu m extragalactic background from the 8 mu m sources, and (5.0 +/- 1.8)% from the 24 mu m sources. At 450 mu m, only the 8 mu m sources within the redshift interval 1 < z < 2 exhibit significant emission with an average flux per source of 3.35 mJy (3.0 sigma). This is a contribution of (37 +/- 12)% to the 450 mu m background. C1 Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Sterrewacht Leiden, NL-233 CA Leiden, Netherlands. Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Inst Astrophys, F-75014 Paris, France. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Dye, S (reprint author), Cardiff Univ, Sch Phys & Astron, 5 The Parade, Cardiff CF24 3YB, Wales. RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Dye, Simon/0000-0002-1318-8343 NR 46 TC 10 Z9 10 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 769 EP 777 DI 10.1086/503863 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100012 ER PT J AU Ashby, MLN Dye, S Huang, JS Eales, S Willner, SP Webb, TMA Barmby, P Rigopoulou, D Egami, E McCracken, H Lilly, S Miyazaki, S Brodwin, M Blaylock, M Cadien, J Fazio, GG AF Ashby, M. L. N. Dye, S. Huang, J. -S. Eales, S. Willner, S. P. Webb, T. M. A. Barmby, P. Rigopoulou, D. Egami, E. McCracken, H. Lilly, S. Miyazaki, S. Brodwin, M. Blaylock, M. Cadien, J. Fazio, G. G. TI Mid-infrared identifications of scuba galaxies in the CUDSS 14 hour field with the Spitzer space telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : formation; galaxies : high-redshift; infrared : galaxies; stars : formation ID DEEP SUBMILLIMETER SURVEY; STAR-FORMING GALAXIES; MULTIBAND IMAGING PHOTOMETER; ARRAY CAMERA IRAC; REDSHIFT SURVEY; INFRARED PROPERTIES; SOURCE EXTRACTION; 1ST-LOOK SURVEY; LOCKMAN HOLE; GROTH STRIP AB We identify 17 possible 8.0 mu m selected counterparts to the submillimeter galaxies in the CUDSS 14 hour field, derived from deep imaging carried out with the IRAC and MIPS instruments aboard the Spitzer Space Telescope. Ten of the 17 counterparts are not the same as those previously identified at shorter wavelengths. We argue that 8.0 mu m selection offers a better means for identifying counterparts to submillimeter galaxies than near-infrared or optical selection. Based on the panchromatic spectral energy distributions (SEDs), most counterparts appear to be powered by ongoing star formation. Power-law fits to the SEDs suggest that five objects in the 8.0 mu m selected counterpart sample harbor dominant active galactic nuclei (AGNs; a sixth object is identified as a possible AGN). The 3.6-8.0 mu m colors of the infrared-selected counterparts are significantly redder than the general IRAC galaxy population in the CUDSS 14 hour field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ Oxford, Dept Astrophys, DWB, Oxford OX1 3RH, England. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Inst Astrophys, F-75014 Paris, France. Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu; jhuang@cfa.harvard.edu; swillner@cfa.harvard.edu; pbarmby@cfa.harvard.edu; gfazio@cfa.harvard.edu RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Dye, Simon/0000-0002-1318-8343 NR 42 TC 28 Z9 28 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 778 EP 791 DI 10.1086/503861 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100013 ER PT J AU Reddy, NA Steidel, CC Fadda, D Yan, L Pettini, M Shapley, AE Erb, DK Adelberger, KL AF Reddy, Naveen A. Steidel, Charles C. Fadda, Dario Yan, Lin Pettini, Max Shapley, Alice E. Erb, Dawn K. Adelberger, Kurt L. TI Star formation and extinction in redshift z similar to 2 galaxies: Inferences from Spitzer MIPS observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dust, extinction; galaxies : evolution; galaxies : high-redshift; galaxies : stellar content; infrared : galaxies ID LYMAN-BREAK GALAXIES; HUBBLE-DEEP-FIELD; X-RAY-PROPERTIES; ULTRALUMINOUS INFRARED GALAXIES; POLYCYCLIC AROMATIC-HYDROCARBON; ULTRAVIOLET LUMINOSITY DENSITY; STELLAR MASS DENSITY; FORMING GALAXIES; SPACE-TELESCOPE; FORMATION RATES AB We use very deep Spitzer MIPS 24 mu m observations to examine the bolometric luminosities (L-bol) and UV extinction properties of more than 200 spectroscopically identified, optically selected (U(n)GR) z similar to 2 galaxies, supplemented with near-IR-selected ("BzK" and "DRG") and submillimeter galaxies at similar redshifts, in the GOODS-N field. Focusing on redshifts 1.5 < z < 2.6, where 24 mu m observations measure the strength of the mid-IR PAH feature, we find that the rest-frame 5-8.5 mu m luminosities (L5-8.5 mu m) are particularly tightly constrained for objects in our sample with precise spectroscopic redshifts. We demonstrate, using stacked X-ray observations and a subset of galaxies with H alpha measurements, that L5-8.5 mu m provides a reliable estimate of L-IR for most star-forming galaxies at z similar to 2. We show that the range of L-IR in the optical/near-IR-selected samples considered extends from similar or equal to 10(10) to > 10(12) L-circle dot, with a mean < L-IR > similar or equal to 2 x 10(11) L-circle dot. Using 24 mu m observations as an independent probe of dust extinction, we find that, as in the local universe, the obscuration L-IR/L-1600 is strongly dependent on L-bol and ranges in value from < 1 to similar to 1000 within the sample considered. However, the obscuration is generally similar to 10 times smaller at a given Lbol at z similar to 2 than at z similar to 0. We show that the values of L-IR and obscuration inferred from the UV spectral slope beta generally agree well with the values inferred from L5-8.5 mu m for L-bol < 10(12) L-circle dot. Using the specific SFRs of galaxies as a proxy for cold gas fraction, we find a wide range in the evolutionary state of galaxies at z similar to 2, from galaxies that have just begun to form stars to those that have already accumulated most of their stellar mass and are about to become, or already are, passively evolving. C1 CALTECH, Astron Opt, Pasadena, CA 91125 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91126 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. McKinsey & Co Inc, Seattle, WA 98101 USA. RP Reddy, NA (reprint author), CALTECH, Astron Opt, MS 105-24, Pasadena, CA 91125 USA. NR 96 TC 228 Z9 228 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 792 EP 812 DI 10.1086/503739 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100014 ER PT J AU Erb, DK Shapley, AE Pettini, M Steidel, CC Reddy, NA Adelberger, KL AF Erb, DK Shapley, AE Pettini, M Steidel, CC Reddy, NA Adelberger, KL TI The mass-metallicity relation at z >= 2 SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : abundances; galaxies : evolution; galaxies : high-redshift ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; EXTRAGALACTIC HII-REGIONS; EMISSION-LINE GALAXIES; HIGH-REDSHIFT GALAXIES; STARBURST GALAXIES; STELLAR POPULATIONS; INTERGALACTIC MEDIUM; METAL ABUNDANCES; SPIRAL GALAXIES AB We use a sample of 87 rest-frame UV-selected star-forming galaxies with mean spectroscopic redshift < z > = 2.26 +/- 0.17 to study the correlation between metallicity and stellar mass at high redshift. Using stellar masses determined from SED fitting to observed 0.3-8 mu m photometry, we divide the sample into six bins in stellar mass and construct six composite H alpha + [N II] spectra from all of the objects in each bin. We estimate the mean oxygen abundance in each bin from the [N II]/H alpha ratio and find a monotonic increase in metallicity with increasing stellar mass, from 12 + log (O/H) < 8.2 for galaxies with < M-star > = 2.7 x 10(9) M-circle dot to 12 + log (O/H) = 8.6 for galaxies with < M-star > = 1.0 x 10(11) M-circle dot. We use the empirical relation between SFR density and gas density to estimate the gas fractions of the galaxies, finding an increase in gas fraction with decreasing stellar mass. These gas fractions, combined with the observed metallicities, allow the estimation of the effective yield y(eff) as a function of stellar mass; in constrast to observations in the local universe, which show a decrease in y(eff) with decreasing baryonic mass, we find a slight increase. Such a variation of metallicity with gas fraction is best fitted by a model with supersolar yield and an outflow rate similar to 4 times higher than the SFR. We conclude that the mass-metallicity relation at high redshift is driven by the increase in metallicity as the gas fraction decreases through star formation and is likely modulated by metal loss from strong outflows in galaxies of all masses. C1 CALTECH, Astron Opt, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Carnegie Observ, Pasadena, CA 91101 USA. RP Erb, DK (reprint author), Harvard Smithsonian Ctr Astrophys, MS 20,60 Garden St, Cambridge, MA 02138 USA. EM derb@cfa.harvard.edu NR 101 TC 631 Z9 631 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 813 EP 828 DI 10.1086/503623 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100015 ER PT J AU Kim, DW Barkhouse, WA Romero-Colmenero, E Green, PJ Kim, M Mossman, A Schlegel, E Silverman, JD Aldcroft, T Anderson, C Ivezic, Z Kashyap, V Tananbaum, H Wilkes, BJ AF Kim, DW Barkhouse, WA Romero-Colmenero, E Green, PJ Kim, M Mossman, A Schlegel, E Silverman, JD Aldcroft, T Anderson, C Ivezic, Z Kashyap, V Tananbaum, H Wilkes, BJ TI Chandra multiwavelength project: Normal galaxies at intermediate redshift SO ASTROPHYSICAL JOURNAL LA English DT Article DE surveys; X-rays : galaxies; X-rays : general ID X-RAY-PROPERTIES; MULTIVARIATE STATISTICAL-ANALYSIS; ACTIVE GALACTIC NUCLEI; STAR-FORMATION HISTORY; FIELD NORTH SURVEY; DEEP FIELD; LUMINOSITY FUNCTION; STARBURST GALAXIES; HELLAS2XMM SURVEY; FORMING GALAXIES AB We have investigated 136 Chandra extragalactic sources, including 93 galaxies with narrow emission lines (NELGs) and 43 with only absorption lines (ALGs). Based on f(X)/f(O), L-X, X-ray spectral hardness, and optical emission-line diagnostics, we have conservatively classified 36 normal galaxies and 71 AGNs. Their redshift ranges from 0.01 to 1.2, with normal galaxies in the range z = 0.01-0.3. Our normal galaxies appear to share characteristics with local galaxies, as expected from the X-ray binary populations and the hot interstellar matter ( ISM). In conjunction with normal galaxies found in other surveys, we found no statistically significant evolution in L-X/L-B, within the limited z range (less than or similar to 0.1). The best-fit slope of our log (N)-log (S) relationship is -1.5 for both S (0.5-2 keV) and B (0.5-8 keV) energy bands, which is considerably steeper than that of the AGN-dominated cosmic background sources, but slightly flatter than the previous estimate, indicating that normal galaxies will not exceed the AGN population until f(X)(0.5-2.0 keV) similar to 2 x 10(-18) ergs s(-1) cm(-2) (a factor of similar to 5 lower than the previous estimate). A group of NELGs appear to be heavily obscured in X-rays. After correcting for intrinsic absorption, their X-ray luminosities could be L-X > 10(44) ergs s(-1), making them type 2 quasar candidates. While most X-ray-luminous ALGs do not appear to be significantly absorbed, we found two heavily obscured objects that could be as luminous as an unobscured broad-line quasar. Among 43 ALGs, we found two E+A galaxy candidates. The X-ray spectra of both galaxies are soft, and one of them has a nearby close companion galaxy, supporting the merger/interaction scenario rather than the dusty starburst hypothesis. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 60 TC 21 Z9 21 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 829 EP 842 DI 10.1086/503828 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100016 ER PT J AU Sakamoto, K Ho, PTP Peck, AB AF Sakamoto, K Ho, PTP Peck, AB TI Imaging molecular gas in the luminous merger NGC 3256: Detection of high-velocity gas and twin gas peaks in the double nucleus SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : individual (NGC 3256); galaxies : interactions; galaxies : ISM; galaxies : starburst; ISM : jets and outflows ID RESOLUTION CO OBSERVATIONS; MASSIVE STAR-FORMATION; INFRARED GALAXIES; NGC 3256; ULTRALUMINOUS GALAXIES; GALACTIC SUPERWINDS; PHYSICAL CONDITIONS; (CO)-C-13 EMISSION; STARBURST GALAXIES; MERGING GALAXIES AB Molecular gas in the merging starburst galaxy NGC 3256 has been imaged with the Submillimeter Array at a resolution of 100; 200 ( 170; 340 pc at 35 Mpc). This is the first interferometric imaging of molecular gas in the most luminous galaxy within z = 0.01. There is a large disk of molecular gas ( r > 3 kpc) in the center of the merger with a strong gas concentration toward the double nucleus. The gas disk having a mass of similar to 3 x 10(9) M-circle dot in the central 3 kpc rotates around a point between the two nuclei that are 850 pc apart on the sky. The molecular gas is warm and turbulent and shows spatial variation of the intensity ratio between CO isotopomers. High-velocity molecular gas is discovered at the galactic center. Its velocity in our line of sight is up to 420 km s(-1) offset from the systemic velocity of the galaxy; the terminal velocity is twice as large as that due to the rotation of the main gas disk. The high-velocity gas is most likely due to a molecular outflow from the gas disk, entrained by the starburst-driven superwind in the galaxy. The molecular outflow is estimated to have a rate of similar to 10 M-circle dot yr(-1) and to play a significant role in the dispersal or depletion of molecular gas from the galactic center. A compact gas concentration and steep velocity gradient are also found around each of the twin nuclei. They are suggestive of a small gas disk rotating around each nucleus. If these are indeed minidisks, their dynamical masses are similar to 10(9) M-circle dot within a radius of 170 pc. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Sakamoto, K (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array,645 N Aohoku Pl, Hilo, HI 96720 USA. EM sakamoto.kazushi@nao.ac.jp NR 95 TC 39 Z9 39 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 862 EP 878 DI 10.1086/503827 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100019 ER PT J AU Rodriguez-Rico, CA Goss, WM Zhao, JH Gomez, Y Anantharamaiah, KR AF Rodriguez-Rico, CA Goss, WM Zhao, JH Gomez, Y Anantharamaiah, KR TI Very large array H53 alpha and H92 alpha line observations of the central region of NGC 253 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : starburst ID RADIO RECOMBINATION LINES; STARBURST GALAXY NGC-253; H II REGIONS; NGC 253; CONTINUUM OBSERVATIONS; VLA OBSERVATIONS; VELOCITY-FIELD; MOLECULAR GAS; IONIZED-GAS; NUCLEUS AB We present new VLA observations toward NGC 253 of the recombination line H53 alpha ( 43 GHz) at an angular resolution of 1.'' 5 x 1.'' 0. The free-free emission at 43 GHz is estimated to be similar to 140 mJy, implying a star formation rate of 2 M-circle dot yr(-1) in the nuclear region of this starburst galaxy. A reanalysis is made for previously reported H92 alpha observations carried out with angular resolution of 1.'' 5 x 1.'' 0 and 0.'' 36 x 0.'' 21. Based on the line and continuum emission models used for the 1.'' 5 x 1.'' 0 angular resolution observations, the RRLs H53 alpha and H92 alpha are tracers of the high-density ( similar to 10(5) cm(-3)) and low-density ( similar to 103 cm(-3)) thermally ionized gas components in NGC 253, respectively. The velocity fields observed in the H53 alpha and H92 alpha lines ( 1.'' 5; 1.'' 0) are consistent. The velocity gradient in the central similar to 18 pc of the NE component, as observed in both the H53 alpha and H92 alpha lines, is in the opposite direction to the velocity gradient determined from the CO observations. The enclosed virial mass, as deduced from the H53 alpha velocity gradient over the NE component, is similar to 5 x 10(6) M-circle dot in the central similar to 18 pc region. The H92 alpha line observations at high angular resolution ( 0.'' 36 x 0.'' 21) reveal a larger velocity gradient, along a P: A: similar to - 45 degrees on the NE component, of similar to 110 km s(-1) arcsec(-1). The dynamical mass estimated using the high angular resolution H92 alpha data ( similar to 7; 106 M-circle dot) supports the existence of an accreted massive object in the nuclear region of NGC 253. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Raman Res Inst, Bangalore 560080, Karnataka, India. RP Rodriguez-Rico, CA (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Campus Morelia,Apartado Postal 3-72, Morelia 58089, Michoacan, Mexico. EM c.rodriguez@astrosmo.unam.mx; mgoss@nrao.edu; jzhao@cfa.harvard.edu; y.gomez@astrosmo.unam.mx RI Anantharamaiah , K. R./E-5369-2012; M, Manjunath/N-4000-2014 OI M, Manjunath/0000-0001-8710-0730 NR 34 TC 22 Z9 22 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 914 EP 923 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100023 ER PT J AU Heng, K McCray, R Zhekov, SA Challis, PM Chevalier, RA Crotts, APS Fransson, C Garnavich, P Kirshner, RP Lawrence, SS Lundqvist, P Panagia, N Pun, CSJ Smith, N Sollerman, J Wang, LF AF Heng, K McCray, R Zhekov, SA Challis, PM Chevalier, RA Crotts, APS Fransson, C Garnavich, P Kirshner, RP Lawrence, SS Lundqvist, P Panagia, N Pun, CSJ Smith, N Sollerman, J Wang, LF TI Evolution of the reverse shock emission from SNR 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; shock waves; supernova remnants; supernovae : individual (SN 1987A) ID SPACE-TELESCOPE OBSERVATIONS; SUPERNOVA REMNANT 1987A; LARGE-MAGELLANIC-CLOUD; VELOCITY LY-ALPHA; CIRCUMSTELLAR RING; X-RAY; LIGHT ECHOES; HOT-SPOTS; H-ALPHA; SN-1987A AB We present new ( 2004 July) G750L and G140L Space Telescope Imaging Spectrograph ( STIS) data of the H alpha and Ly alpha emission from supernova remnant ( SNR) 1987A. With the aid of earlier data, from 1997 October to 2002 October, we track the local evolution of Ly alpha emission and both the local and global evolution of H alpha emission. The most recent observations allow us to directly compare the H alpha and Ly alpha emission from the same slit position and at the same epoch. Consequently, we find clear evidence that, unlike H alpha, Ly alpha is reflected from the debris by resonant scattering. In addition to emission that we can clearly attribute to the surface of the reverse shock, we also measure comparable emission, in both H alpha and Ly alpha, that appears to emerge from supernova debris interior to the surface. New observations taken through slits positioned slightly eastward and westward of a central slit show a departure from cylindrical symmetry in the H alpha surface emission. Using a combination of old and new observations, we construct a light curve of the total H alpha flux, F, from the reverse shock, which has increased by a factor of similar to 4 over about 8 yr. However, due to large systematic uncertainties, we are unable to discern between the two limiting behaviors of the flux: F proportional to t ( self-similar expansion) and F proportional to t(5) ( halting of the reverse shock). Such a determination is important for constraining the rate of hydrogen atoms crossing the shock, which is relevant to the question of whether the reverse shock emission will vanish in less than or similar to 7 yr. Future deep, low- or moderate-resolution spectra are essential for accomplishing this task. C1 Univ Colorado, JILA, Boulder, CO 80309 USA. Bulgarian Acad Sci, Space Res Inst, BU-1000 Sofia, Bulgaria. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Stockholm Observ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. 151 Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11590 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hong Kong, Dept Phys, Hong Kong, Peoples R China. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. EO Lawrence Berkeley Natl Lab, Inst Nucl & Particle Phys, Berkeley, CA 94720 USA. RP Heng, K (reprint author), Univ Colorado, JILA, 440 UCB, Boulder, CO 80309 USA. EM hengk@colorado.edu; dick@jila.colorado.edu OI Sollerman, Jesper/0000-0003-1546-6615 NR 36 TC 23 Z9 24 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 959 EP 970 DI 10.1086/503896 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100027 ER PT J AU Heinke, CO Rybicki, GB Narayan, R Grindlay, JE AF Heinke, Craig O. Rybicki, George B. Narayan, Ramesh Grindlay, Jonathan E. TI A hydrogen atmosphere spectral model applied to the neutron star X7 in the globular cluster 47 tucanae SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (NGC 104); radiative transfer; stars : neutron; X-rays : binaries ID EQUATION-OF-STATE; THERMAL EMISSION; INTERSTELLAR-MEDIUM; GLOBULAR-CLUSTERS; RX J185635-3754; RAY-SPECTRA; AQUILA X-1; XMM-NEWTON; QUIESCENCE; PULSAR AB Current X-ray missions are providing high-quality X-ray spectra from neutron stars ( NSs) in quiescent low-mass X-ray binaries ( qLMXBs). This has motivated us to calculate new hydrogen atmosphere models, including opacity due to free-free absorption and Thomson scattering, thermal electron conduction, and self-irradiation by photons from the compact object. We have constructed a self-consistent grid of neutron star models covering a wide range of surface gravities, as well as effective temperatures, which we make available to the scientific community. We present multiepoch Chandra X-ray observations of the qLMXB X7 in the globular cluster 47 Tuc, which is remarkably nonvariable on timescales from minutes to years. Its high-quality X-ray spectrum is adequately fitted by our hydrogen atmosphere model without any hard power-law component or narrow spectral features. If a mass of 1.4 M-circle dot is assumed, our spectral fits require that its radius be in the range R-ns =(+1.8)(-1.6) km ( 90% confidence), which is larger than that expected from currently preferred models of NS interiors. If its radius is assumed to be 10 km, then a mass of M-ns = 2.20(-0.16)(+0.03) M-circle dot is required. Using models with the appropriate surface gravity for each value of the mass and radius becomes important for interpretation of the highest quality data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heinke, CO (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM cheinke@northwestern.edu; grybicki@cfa.harvard.edu; rnarayan@cfa.harvard.edu; jgrindlay@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730; Heinke, Craig/0000-0003-3944-6109 NR 56 TC 152 Z9 152 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 JUN 20 PY 2006 VL 644 IS 2 BP 1090 EP 1103 DI 10.1086/503701 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100037 ER PT J AU Boden, AF Torres, G Latham, DW AF Boden, Andrew F. Torres, Guillermo Latham, David W. TI A physical orbit for the high proper motion binary HD 9939 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : abundances; stars : fundamental parameters; stars : individual (HD 9939) ID PALOMAR TESTBED INTERFEROMETER; LINED SPECTROSCOPIC BINARIES; AGE-METALLICITY RELATION; MILKY-WAY DISK; CHEMICAL ENRICHMENT; SOLAR NEIGHBORHOOD; RADIAL-VELOCITIES; Y-2 ISOCHRONES; STAR-FORMATION; 12 BOOTIS AB We report spectroscopic and interferometric observations of the high proper motion double-lined binary system HD 9939, with an orbital period of approximately 25 days. By combining our radial-velocity and visibility measurements, we estimate the system physical orbit and derive dynamical masses for the components of MA 1.072 +/- 0.014 M(circle dot) and M(B) 0.8383 +/- 0.0081 M(circle dot), with fractional errors of 1.3% and 1.0%, respectively. We also determine a system distance of 42.23 +/- 0.21 pc, corresponding to an orbital parallax of orb 23.68 +/- 0.12 mas. The system distance and the estimated brightness difference between the stars in V, H, and K yield component absolute magnitudes in these bands. By spectroscopic analysis and spectral energy distribution modeling, we also estimate the component effective temperatures and luminosities as T(eff)(A) 5050 +/- 100 K and T(eff)(B) 4950 +/- 200 K and LA 2.451 +/- 0: 041 L(circle dot) and L(B) 0.424 +/- 0.023 L(circle dot). Both our spectral analysis and comparison with stellar models suggest that HD 9939 has elemental abundances near solar values. Further, comparison with stellar models suggests that the HD 9939 primary has evolved off the main sequence and appears to be traversing the Hertzsprung gap as it approaches the red giant phase of its evolution. Our measurements of the primary properties provide new empirical constraints on stellar models during this particularly dynamic evolutionary phase. That HD 9939 is currently in a relatively short lived evolutionary state allows us to estimate the system age as 9.12 +/- 0.25 Gyr. In turn, the age and abundance of the system place a potentially interesting, if anecdotal, constraint on star formation in the Galactic disk. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Boden, AF (reprint author), CALTECH, Michelson Sci Ctr, 770 S Wilson Ave, Pasadena, CA 91125 USA. NR 40 TC 24 Z9 25 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 JUN 20 PY 2006 VL 644 IS 2 BP 1193 EP 1201 DI 10.1086/503793 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100045 ER PT J AU O'Donovan, FT Charbonneau, D Torres, G Mandushev, G Dunham, EW Latham, DW Alonso, R Brown, TM Esquerdo, GA Everett, ME Creevey, OL AF O'Donovan, FT Charbonneau, D Torres, G Mandushev, G Dunham, EW Latham, DW Alonso, R Brown, TM Esquerdo, GA Everett, ME Creevey, OL TI Rejecting astrophysical false positives from the tres transiting planet survey: The example of GSC 03885-00829 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; planetary systems; stars : individual (GSC 03885-00829); techniques : photometric; techniques : radial velocities ID LOW-MASS STARS; EXTRASOLAR PLANET; SEARCH; PHOTOMETRY; CANDIDATES; ATMOSPHERE; TELESCOPE; ALGORITHM; CATALOG; COLORS AB Ground-based wide-field surveys for nearby transiting gas giants are yielding far fewer true planets than astrophysical false positives, some of which are difficult to reject. Recent experience has highlighted the need for careful analysis to eliminate astronomical systems in which light from a faint eclipsing binary is blended with that from a bright star. During the course of the Transatlantic Exoplanet Survey, we identified a system presenting a transit-like periodic signal. We obtained the proper motion and infrared color of this target (GSC 03885 - 00829) from publicly available catalogs, which suggested this star is an F dwarf, supporting our transit hypothesis. This spectral classification was confirmed using spectroscopic observations from which we determined the stellar radial velocity. The star did not exhibit any signs of a stellar mass companion. However, subsequent multicolor photometry displayed a color-dependent transit depth, indicating that a blend was the likely source of the eclipse. We successfully modeled our initial photometric observations of GSC 03885 - 00829 as the light from a K dwarf binary system superimposed on the light from a late F dwarf star. High-dispersion spectroscopy confirmed the presence of light from a cool stellar photosphere in the spectrum of this system. With this candidate, we demonstrate both the difficulty in identifying certain types of false positives in a list of candidate transiting planets and our procedure for rejecting these imposters, which may be useful to other groups performing wide-field transit surveys. C1 CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lowell Observ, Flagstaff, AZ 86001 USA. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. Planetary Sci Inst, Tucson, AZ 85719 USA. RP O'Donovan, FT (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM ftod@caltech.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 NR 46 TC 43 Z9 43 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2006 VL 644 IS 2 BP 1237 EP 1245 DI 10.1086/503740 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XS UT WOS:000238340100050 ER PT J AU Guerova, G Bey, I Attie, JL Martin, RV Cui, J Sprenger, M AF Guerova, G. Bey, I. Attie, J. -L. Martin, R. V. Cui, J. Sprenger, M. TI Impact of transatlantic transport episodes on summertime ozone in Europe SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID UNITED-STATES; SURFACE OZONE; INTERCONTINENTAL TRANSPORT; TROPOSPHERIC OZONE; ART.; MODEL; POLLUTION; STRATOSPHERE; CLIMATOLOGY; VARIABILITY AB This paper reports on the transport of ozone (O-3) and related species over the North Atlantic ocean and its impact on Europe. Measurements of nitrogen dioxide (NO2) and carbon monoxide (CO) columns from the GOME and MOPITT satellite instruments, respectively, are used in conjunction with the GEOS-CHEM global model of transport and tropospheric chemistry to identify the major events of long range transport that reach Europe over the course of summer 2000. Sensitivity model simulations are used to analyse observed O-3 distributions with respect to the impact of long range transport events. For that purpose, we used in- situ O-3 observations taken at the mountain site of Jungfraujoch as well as O-3 vertical profiles taken in the vicinity of central European cities. Over the course of summer 2000, we identified 9 major episodes of transatlantic pollution transport; 7 events are associated with transient cyclones while 2 events occur through zonal transport ( e. g. by advection in the strong low-level westerly winds established in summer between the Azores anticyclone and transient cyclones). We find that on average three episodes occur per month with the strongest ones being in June. The number and frequency of long range transport events that reach Europe are driven by the position and strength of the Azores anticyclone. Model sensitivity simulations indicate that the summer mean North American O-3 contribution ranges from 3 to 5 ppb ( 7 - 11%) in the planetary boundary layer and 10 to 13 ppb ( 18 - 23%) in the middle and upper troposphere. During particular episodes, North American sources can result in O3 enhancements up to 25 - 28 ppb in the layer between 800 - 600 hPa and 10 - 12 ppb in the boundary layer. The impact of the zonal transport events on O-3 distribution over Europe is more clearly seen below 700 hPa as they tend to transport pollution at lower levels while the events associated with transient cyclones are more likely to have an impact on the middle and upper troposphere (i.e. above 600 hPa). The air mass origins found in the GEOS-CHEM model are clearly confirmed by back trajectory analyses. During most of the 9 events, a strong contribution in North American O-3 is in general associated with only little European O-3 and vice-versa ( in particular at the Jungfraujoch). A substantial North American contribution (e.g., 30% or higher) to O-3 over Europe does not always result in pronounced O-3 enhancements in the observations during our period of study. C1 Ecole Polytech Fed Lausanne, Lab Modelisat Chim Atmospher, Lausanne, Switzerland. Observ Midi Pyrenees, Lab Aerol, F-31400 Toulouse, France. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Zurich, Switzerland. RP Guerova, G (reprint author), Ecole Polytech Fed Lausanne, Lab Modelisat Chim Atmospher, Lausanne, Switzerland. EM guergana.guerova@epfl.ch RI Martin, Randall/A-2051-2008; Guerova, Guergana/D-1943-2013; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 40 TC 32 Z9 32 U1 1 U2 11 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD JUN 20 PY 2006 VL 6 BP 2057 EP 2072 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 054SC UT WOS:000238397900002 ER PT J AU Page, RA Ryan, MJ AF Page, Rachel A. Ryan, Michael J. TI Social transmission of novel foraging behavior in bats: Frog calls and their referents SO CURRENT BIOLOGY LA English DT Article ID INFORMATION-TRANSFER; ECHOLOCATION CALLS; CHIROPTERA; PREDATION; FOOD; EXTINCTIONS; MECHANISMS; ANIMALS; DISEASE AB The fringe-lipped bat, Trachops cirrhosus, uses prey-emitted acoustic cues (frog calls) to assess prey palatability [1]. Previous experiments show that wild T. cirrhosus brought into the laboratory are flexible in their ability to reverse the associations they form between prey cues and prey quality [2]. Here we asked how this flexibility can be achieved in nature. We quantified the rate at which bats learned to associate the calls of a poisonous toad species with palatable prey by placing bats in three groups: (a) social learning, in which a bat inexperienced with the novel association was allowed to observe an experienced bat; (b) social facilitation, in which two inexperienced bats were presented with the experimental task together; and (c) trial-and-error, in which a single inexperienced bat was presented with the experimental task alone. In the social-learning group, bats rapidly acquired the novel association in an average of 5.3 trials. In the social-facilitation and trial-and-error groups, most bats did not approach the call of the poisonous species after 100 trials. Thus, once acquired, novel associations between prey cue and prey quality could spread rapidly through the bat population by cultural transmission. This is the first case to document predator social learning of an acoustic prey cue. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Page, RA (reprint author), Univ Texas, Sect Integrat Biol, Univ Stn C0930, Austin, TX 78712 USA. EM rachelpage@mail.utexas.edu NR 40 TC 40 Z9 40 U1 4 U2 20 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD JUN 20 PY 2006 VL 16 IS 12 BP 1201 EP 1205 DI 10.1016/j.cub.2006.04.038 PG 5 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 057LP UT WOS:000238597600023 PM 16782010 ER PT J AU Zug, GR Allison, A AF Zug, George R. Allison, Allen TI New Carlia fusca complex lizards (Reptilia : Squamata : Scincidae) from New Guinea, Papua-Indonesia SO ZOOTAXA LA English DT Article DE Squamata; Scincidae; Carlia fusca; Papua-Indonesia; New Guinea; geographic variation; new species AB Recent rapid-assessment surveys in western New Guinea have provided well-documented voucher specimens that show greater speciation within the Carlia fusca complex in this area than indicated by the examination of older museum specimens. Variation in the morphometric and scalation traits of these new species does not differ greatly from other fusca complex species. This result was anticipated owing to the overall low level of variation in these morphological features in the fusca complex. Regionalization of distinct color patterns and abrupt shifts from one pattern to another indicate the existence of a distinct species along much of the southern coast from the Eilanden River basin to Etna Bay and another species from the northern coast of the Bomberai Peninsula. The variation and distribution of fusca complex species are examined for populations in the southern and western "mainland" Papua-Indonesia. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Bernice P Bishop Museum, Dept Nat Sci, Honolulu, HI 96817 USA. RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM zugg@si.edu; allison@hawaii.edu NR 10 TC 4 Z9 4 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 19 PY 2006 IS 1237 BP 27 EP 44 PG 18 WC Zoology SC Zoology GA 062YX UT WOS:000238984000003 ER PT J AU Marinoni, L Mathis, WN AF Marinoni, Luciane Mathis, Wayne N. TI A cladistic analysis of the Neotropical genus Sepedonea Steyskal (Diptera : Sciomyzidae) SO ZOOTAXA LA English DT Article DE Sciomyzidae; Sepedonea; Neotropical; cladistic analysis ID BIOLOGICAL-CONTROL; LIVER FLUKE; SNAIL; AGENT AB A cladistic analysis of the 13 known species of Sepedonea Steyskal, 1973, is presented and a new species, Sepedonea giovana sp. n., is described. The monophyly of the genus is confirmed, as is the genus' sister-group relationship to Sepedomerus Steyskal, 1973. The cladistic analysis was done using NONA and a matrix of 27 adult morphological characters, including structures of the male and female terminalia. The relationships in parenthetic notation are: ( S. guatemalana ( S. veredae ( S. lindneri ( S. isthmi ( S. lagoa (( S. barbosai+ S. canabravana) (( S. neffi ( S. giovana+ S. guianica))( S. telson ( S. incipiens+ S. trichotypa))))))))). C1 Univ Fed Parana, Dept Zool, BR-81531990 Curitiba, Parana, Brazil. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Marinoni, L (reprint author), Univ Fed Parana, Dept Zool, Caixa Postal 19020, BR-81531990 Curitiba, Parana, Brazil. EM lmarinoni@ufpr.br; mathisw@si.edu RI Marinoni, Luciane /C-5720-2013 NR 21 TC 3 Z9 3 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 JUN 19 PY 2006 IS 1236 BP 37 EP 52 PG 16 WC Zoology SC Zoology GA 062YV UT WOS:000238983800003 ER PT J AU Buffington, ML AF Buffington, Matthew L. TI The description of Moritiella Buffington, new genus (Hymenoptera : Figitidae : Eucoilinae) SO ZOOTAXA LA English DT Article DE Moritiella; Zaeucoila group; Eucoilinae; Figitidae; Cynipoidea; new species; new genus ID CYNIPOIDEA; PHYLOGENY AB The genus Moritiella Buffington, n. gen., is described, diagnosed and illustrated ( Hymenoptera: Figitidae: Eucoilinae). Two species new to science are described: M. elegans n. sp. and M. astrudae n. sp. Phylogenetic evidence suggests Moritiella is among the Zaeucoila group of genera, a group of eucoilines chiefly parasitic upon leaf-mining Agromyzidae ( Diptera). C1 Univ Calif Riverside, Dept Entomol, Riverside, CA 92521 USA. RP Buffington, ML (reprint author), USDA, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, 10 & Constitut Ave NW, Washington, DC 20013 USA. NR 7 TC 5 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 JUN 19 PY 2006 IS 1237 BP 61 EP 68 PG 8 WC Zoology SC Zoology GA 062YX UT WOS:000238984000005 ER PT J AU Canty, T Pickett, HM Salawitch, RJ Jucks, KW Traub, WA Waters, JW AF Canty, T Pickett, HM Salawitch, RJ Jucks, KW Traub, WA Waters, JW TI Stratospheric and mesospheric HOx: results from aura MLS and FIRS-2 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VIBRATIONALLY EXCITED MOLECULES; O-3 DEFICIT PROBLEM; MIDDLE ATMOSPHERE; OZONE; OH; DILEMMA; RADICALS; CLUE; H2O AB Observations of OH and HO2 from Aura MLS for four seasons and diurnal profiles from the FIRS-2 balloon instrument for Fall 2004 are compared with photochemical model simulations testing three sets of kinetics parameters. MLS and FIRS-2 OH profiles, between 25 - 60 km, are lower than model results using standard kinetics. Use of a faster, previously published rate constant for O+OH leads to better agreement with MLS and FIRS-2 profiles of OH. A 20% increase in the rate of HO2+ OH and the faster rate for O+ OH results in improved overall agreement with observations of OH, HO2, HOx, and HO2/OH. Since the MLS and FIRS-2 observations of HOx are reasonably well described by these models, they are therefore not consistent with the previously reported HOx dilemma. However, all models considered here result in calculated odd oxygen loss exceeding production, consistent with the long standing ozone deficit problem. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Canty, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-601, Pasadena, CA 91109 USA. EM tcanty@jpl.nasa.gov RI Salawitch, Ross/B-4605-2009; Canty, Timothy/F-2631-2010 OI Salawitch, Ross/0000-0001-8597-5832; Canty, Timothy/0000-0003-0618-056X NR 14 TC 23 Z9 23 U1 0 U2 2 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 JUN 17 PY 2006 VL 33 IS 12 AR L12802 DI 10.1029/2006GL025964 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 057BO UT WOS:000238570100003 ER PT J AU Bleidorn, C Kruse, I Albrecht, S Bartolomaeus, T AF Bleidorn, Christoph Kruse, Inken Albrecht, Sylvia Bartolomaeus, Thomas TI Mitochondrial sequence data expose the putative cosmopolitan polychaete Scoloplos armiger (Annelida, Orbiniidae) as a species complex SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID MOLECULAR-DATA; GENE ORDER; RAPD-PCR; SEA; GENOMES; POPULATIONS; SYSTEMATICS; SPECIATION; SEDIMENTS; MODEL AB Background: Polychaetes assigned as Scoloplos armiger (Orbiniidae) show a cosmopolitan distribution and have been encountered in all zoogeographic regions. Sibling S. armiger- like species have been revealed by recent studies using RAPDs and AFLP genetic data. We sequenced a similar to 12 kb fragment of the Scoloplos cf. armiger mitochondrial genome and developed primers for variable regions including the 3' end of the cox3 gene, trnQ, and most of nad6. A phylogenetic analysis of this 528-nucleotide fragment was carried out for S. armiger- like individuals from the Eastern North Atlantic as well as Pacific regions. The aim of this study is to test the cosmopolitan status, as well as to clarify the systematics of this species complex in the Eastern North Atlantic, while using a few specimens from the Pacific Ocean for comparision. Results: Phylogenetic analysis of the cox3-trnQ-nad6 data set recovered five different clades of Scoloplos cf. armiger. The fragment of the mitochondrial genome of Scoloplos cf. armiger is 12,042 bp long and contains 13 protein coding genes, 15 of the 22 expected tRNAs, and the large ribosomal subunit (rrnl). Conclusion: The sequenced cox3-trnQ-nad6 fragment proved to be very useful in phylogenetic analyses of Scoloplos cf. armiger. Due to its larger sampling scale this study goes beyond previous analyses which used RAPD and AFLP markers. The results of this study clearly supports that Scoloplos armiger represents a species complex and not a cosmopolitan species. We find at least two S. armiger- like species within the Pacific region and three different S. armiger- like species in the North Atlantic. Implications for the taxonomy and the impact on ecological studies are discussed. C1 Free Univ Berlin, Inst Zool, D-14195 Berlin, Germany. Univ Potsdam, Inst Biochem & Biol, Unit Evolutionary Biol Systemat Zool, D-14476 Potsdam Golm, Germany. Inst Zoo & Wildlife Res, D-10252 Berlin, Germany. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. RP Bleidorn, C (reprint author), Free Univ Berlin, Inst Zool, Koenigin Luise Str 1-3, D-14195 Berlin, Germany. EM bleidorn@uni-potsdam.de; inkenkruse@web.de; sylvia-albrecht@arcor.de; tbartol@zoosyst-berlin.de RI Kruse, Inken/G-2624-2013; Kruse, Inken/E-4207-2014; Kruse, Inken/B-5949-2016; OI Bleidorn, Christoph/0000-0001-7295-6616 NR 56 TC 30 Z9 30 U1 0 U2 13 PU BIOMED CENTRAL LTD PI LONDON PA MIDDLESEX HOUSE, 34-42 CLEVELAND ST, LONDON W1T 4LB, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUN 15 PY 2006 VL 6 AR 47 DI 10.1186/1471-2148/6/47 PG 13 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 075SX UT WOS:000239906600001 PM 16776822 ER PT J AU Dmitrieva, NI Ferraris, JD Norenburg, JL Burg, MB AF Dmitrieva, NI Ferraris, JD Norenburg, JL Burg, MB TI The saltiness of the sea breaks DNA in marine invertebrates - Possible implications for animal evolution SO CELL CYCLE LA English DT Article DE NaCl; DNA damage; evolution; cambrian explosion; osmoregulation; marine invertabrates ID MURINE KIDNEY-CELLS; CAMBRIAN EXPLOSION; HIGH NACL; HYPEROSMOLALITY; STRESS; SALT; UREA AB More than 97 percent of the world's water is ocean and its average osmolality of 1000 mosmol/kg is much higher than the 300 mosmol/kg found in most of the intercellular fluids of vertebrates. Many marine invertebrates are osmoconformers, meaning that the osmolality of their extracellular fluid is the same as that of seawater. We report here that marine invertebrates from diverse phyla have numerous DNA breaks in their cells while they are exposed to normal seawater containing high NaCl, but that the DNA breaks decrease or disappear when the animals are acclimated to the same water diluted to 300 mosmol/kg. We speculate that, since DNA breaks cause mutations, salinity might have important background effects on the rate and course of evolution. C1 NHLBI, Kidney & Electrolyte Metab Lab, NIH, Bethesda, MD 20892 USA. Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC USA. RP Dmitrieva, NI (reprint author), 9000 Rockville Pike,Bldg 10,Rm 6N260, Bethesda, MD 20892 USA. EM dmitrien@nhlbi.nih.gov RI Dmitrieva, Natalia/A-2924-2013; Norenburg, Jon/K-3481-2015 OI Dmitrieva, Natalia/0000-0001-8074-6950; Norenburg, Jon/0000-0001-7776-1527 FU Intramural NIH HHS NR 24 TC 14 Z9 14 U1 2 U2 9 PU LANDES BIOSCIENCE PI GEORGETOWN PA 810 SOUTH CHURCH STREET, GEORGETOWN, TX 78626 USA SN 1538-4101 J9 CELL CYCLE JI Cell Cycle PD JUN 15 PY 2006 VL 5 IS 12 BP 1320 EP 1323 DI 10.4161/cc.5.12.2867 PG 4 WC Cell Biology SC Cell Biology GA 057FH UT WOS:000238581200016 PM 16775417 ER PT J AU Mccoy, TJ Ketcham, RA Wilson, L Benedix, GK Wadhwa, M Davis, AM AF McCoy, Timothy J. Ketcham, Richard A. Wilson, Lionel Benedix, Gretchen K. Wadhwa, Meenakshi Davis, Andrew M. TI Formation of vesicles in asteroidal basaltic meteorites SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE basalts; vesicles; asteroids; meteorites; volatiles ID PARENT BODY; ERUPTIONS; EUCRITE; IBITIRA; DIFFERENTIATION; GEOCHEMISTRY; PETROLOGY; MODEL AB Rare asteroidal vesicular basalts have previously been thought to form in surficial lava flows with CO as the vesicle-forming gas. However, vesicular lava flows are unlikely on small, airless bodies such as asteroids. To unravel the origin of these rocks, we analyzed vesicle sizes and abundances for two angrites and two eucrites using high-resolution X-ray computed tomography and conducted numerical modeling of bubble formation in a dike of ascending magma. Modeling results indicate that thin (< 30 cm wide) dikes are trapped at similar to 5 km depth where similar to 75 ppm of CO and CO2 contribute equally to vesicle formation. Vesicular eucrites were metamorphosed in this deep-seated environment, the gas was lost, and they were excavated by impacts. Published by Elsevier B.V. C1 Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Univ Lancaster, Div Environm Sci, Lancaster LA1 4YQ, England. Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Nat Hist Museum, Dept Mineral, London SW7 5BD, England. Field Museum Nat Hist, Dept Geol, Chicago, IL 60605 USA. Univ Chicago, Chicago Ctr Cosmochem, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Dept Geophys Sci, Chicago, IL 60637 USA. RP Mccoy, TJ (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. EM mccoyt@si.edu RI Ketcham, Richard/B-5431-2011; OI Ketcham, Richard/0000-0002-2748-0409; Davis, Andrew/0000-0001-7955-6236; Benedix, Gretchen/0000-0003-0990-8878 NR 34 TC 19 Z9 19 U1 3 U2 11 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 JUN 15 PY 2006 VL 246 IS 1-2 BP 102 EP 108 DI 10.1016/j.epsl.2006.04.002 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 066AE UT WOS:000239200800008 ER PT J AU Mavarez, J Salazar, CA Bermingham, E Salcedo, C Jiggins, CD Linares, M AF Mavarez, J Salazar, CA Bermingham, E Salcedo, C Jiggins, CD Linares, M TI Speciation by hybridization in Heliconius butterflies SO NATURE LA English DT Article ID HOMOPLOID HYBRID SPECIATION; MELPOMENE LINNAEUS; MIMICRY; EVOLUTION; POPULATION; SELECTION; ORIGIN; CYDNO AB Speciation is generally regarded to result from the splitting of a single lineage. An alternative is hybrid speciation, considered to be extremely rare, in which two distinct lineages contribute genes to a daughter species. Here we show that a hybrid trait in an animal species can directly cause reproductive isolation. The butterfly species Heliconius heurippa is known to have an intermediate morphology and a hybrid genome(1), and we have recreated its intermediate wing colour and pattern through laboratory crosses between H. melpomene, H. cydno and their F-1 hybrids. We then used mate preference experiments to show that the phenotype of H. heurippa reproductively isolates it from both parental species. There is strong assortative mating between all three species, and in H. heurippa the wing pattern and colour elements derived from H. melpomene and H. cydno are both critical for mate recognition by males. C1 Univ Los Andes, Inst Genet, Bogota, Colombia. Smithsonian Trop Res Inst, Panama City, Panama. Univ Edinburgh, Sch Biol Sci, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. RP Mavarez, J (reprint author), Univ Los Andes, Inst Genet, Carrera 1E 18a-10,POB 4976, Bogota, Colombia. EM mavarezj@sl.edu RI Jiggins, Chris/B-9960-2008; Salazar, camilo/A-1647-2010; Linares, Mauricio/I-3509-2016 OI Jiggins, Chris/0000-0002-7809-062X; Salazar, camilo/0000-0001-9217-6588; Linares, Mauricio/0000-0002-1021-0226 NR 29 TC 213 Z9 228 U1 8 U2 125 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 15 PY 2006 VL 441 IS 7095 BP 868 EP 871 DI 10.1038/nature04738 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 052SL UT WOS:000238254100041 PM 16778888 ER PT J AU Ates, C Pohl, T Pattard, T Rost, JM AF Ates, C Pohl, T Pattard, T Rost, JM TI Strong interaction effects on the atom counting statistics of ultracold Rydberg gases SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article AB Based on simple rate equations for the Rydberg excitation process, we are able to model microscopically the dynamics of Rydberg excitation in ensembles of a large number of ultracold atoms, which is beyond the capabilities of fully ab initio approaches. Our results for the distribution of Rydberg atom numbers are in good agreement with recent experimental data, confirming the quenching of the distribution caused by Rydberg-Rydberg interactions. C1 Harvard Univ, Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Ates, C (reprint author), Max Planck Inst Phys Complex Syst, Nothnitzer Str 38, D-01187 Dresden, Germany. EM cenap@mpipks-dresden.mpg.de RI Pohl, Thomas/B-5133-2013; OI Pattard, Thomas/0000-0002-2276-5173; Rost, Jan M./0000-0002-8306-1743 NR 7 TC 48 Z9 48 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUN 14 PY 2006 VL 39 IS 11 BP L233 EP L239 DI 10.1088/0953-4075/39/11/L02 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 054LP UT WOS:000238378500002 ER PT J AU Elosegui, P Davis, JL Oberlander, D Baena, R Ekstrom, G AF Elosegui, P. Davis, J. L. Oberlander, D. Baena, R. Ekstrom, G. TI Accuracy of high-rate GPS for seismology SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GLOBAL POSITIONING SYSTEM; EARTHQUAKE; MOTIONS AB We built a device for translating a GPS antenna on a positioning table to simulate the ground motions caused by an earthquake. The earthquake simulator is accurate to better than 0.1 mm in position, and provides the "ground truth" displacements for assessing the technique of high-rate GPS. We found that the root-mean-square error of the 1-Hz GPS position estimates over the 15-min duration of the simulated seismic event was 2.5 mm, with approximately 96% of the observations in error by less than 5 mm, and is independent of GPS antenna motion. The error spectrum of the GPS estimates is approximately flicker noise, with a 50% decorrelation time for the position error of similar to 1.6 s. We find that, for the particular event simulated, the spectrum of surface deformations exceeds the GPS error spectrum within a finite band. More studies are required to determine whether a generally optimal bandwidth exists for a target group of seismic events. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, IEEC, Inst Space Sci, E-08034 Barcelona, Spain. MIT, Lincoln Lab, Lexington, MA 02420 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Elosegui, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. EM pelosegui@cfa.harvard.edu; jdavis@cfa.harvard.edu; oberlander@ll.mit.edu; rbaena@ieec.fcr.es; ekstrom@eps.harvard.edu RI Ekstrom, Goran/C-9771-2012; Davis, James/D-8766-2013 OI Ekstrom, Goran/0000-0001-6410-275X; Davis, James/0000-0003-3057-477X NR 15 TC 33 Z9 37 U1 0 U2 1 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 JUN 13 PY 2006 VL 33 IS 11 AR L11308 DI 10.1029/2006GL026065 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 057BK UT WOS:000238569700002 ER PT J AU Medina, M Collins, AG Takaoka, TL Kuehl, JV Boore, JL AF Medina, M Collins, AG Takaoka, TL Kuehl, JV Boore, JL TI Naked corals: Skeleton loss in Scleractinia SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID ANEMONE METRIDIUM-SENILE; GROUP-I INTRONS; MITOCHONDRIAL GENOME; MOLECULAR EVOLUTION; CNIDARIA; ANTHOZOA; CONTAINS; HISTORY; GENE; SYSTEMATICS AB Stony corals, which form the framework for modern reefs, are classified as Scleractinia (Cnidaria, Anthozoa, and Hexacorallia) in reference to their external aragonitic skeletons. However, persistent notions, collectively known as the "naked coral" hypothesis, hold that the scleractinian skeleton does not define a natural group. Three main lines of evidence have suggested that some stony corals are more closely related to one or more of the soft-bodied hexacorallian groups than they are to other scleractinians: (i) morphological similarities; (it) lack of phylogenetic resolution in molecular analyses of scleractinians; and (iii) discrepancy between the commencement of a diverse scleractinian fossil record at 240 million years ago (Ma) and a molecule-based origination of at least 300 Ma. No molecular evidence has been able to clearly reveal relationships at the base of a well supported clade composed of scleractinian lineages and the nonskeletonized Corallimorpharia. We present complete mitochondrial genome data that provide strong evidence that one clade of scleractinians is more closely related to Corallimorpharia than it is to a another clade of scleractinians. Thus, the scleractinian skeleton, which we estimate to have originated between 240 and 288 Ma, was likely lost in the ancestry of Corallimorpharia. We estimate that Corallimorpharia originated between 110 and 132 Ma during the late- to mid-Cretaceous, coinciding with high levels of oceanic CO2, which would have impacted aragonite solubility. Corallimorpharians escaped extinction from aragonite skeletal dissolution, but some modern stony corals may not have such fortunate fates under the pressure of increased anthropogenic CO2 in the ocean. C1 Joint Genome Inst, Dept Energy, Dept Evolutionary Genom, Walnut Creek, CA 94598 USA. NOAA, Fisheries Serv, Natl Systemat Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Medina, M (reprint author), Univ Calif, Sch Nat Sci, POB 2039, Merced, CA 95344 USA. EM mmedina@ucmerced.edu RI Collins, Allen/A-7944-2008 OI Collins, Allen/0000-0002-3664-9691 NR 36 TC 143 Z9 147 U1 4 U2 26 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUN 13 PY 2006 VL 103 IS 24 BP 9096 EP 9100 DI 10.1073/pnas.0602444103 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 054ID UT WOS:000238369100037 PM 16754865 ER PT J AU Cackett, EM Wijnands, R Heinke, CO Pooley, D Lewin, WHG Grindlay, JE Edmonds, PD Jonker, PG Miller, JM AF Cackett, EM Wijnands, R Heinke, CO Pooley, D Lewin, WHG Grindlay, JE Edmonds, PD Jonker, PG Miller, JM TI A Chandra X-ray observation of the globular cluster Terzan 1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : X 1732-304; stars : neutron; globular clusters : individual : Terzan 1; X-rays : binaries ID NEUTRON-STAR; GALACTIC-CENTER; BURST SOURCES; TRANSIENTS; CATALOG; BINARIES; NGC-6440; COUNTERPARTS; VARIABILITY; QUIESCENCE AB We present a similar to 19-ks Chandra Advanced CCD Imaging Spectrometer (ACIS)-S observation of the globular cluster Terzan 1. 14 sources are detected within 1.4 arcmin of the cluster centre with two of these sources predicted to be not associated with the cluster (background active galactic nuclei or foreground objects). The neutron star X-ray transient, X1732-304, has previously been observed in outburst within this globular cluster with the outburst seen to last for at least 12 yr. Here, we find four sources that are consistent with the ROSAT position for this transient, but none of the sources are fully consistent with the position of a radio source detected with the Very Large Array that is likely associated with the transient. The most likely candidate for the quiescent counterpart of the transient has a relatively soft spectrum and an unabsorbed 0.5-10 keV luminosity of 2.6 x 10(32) erg s(-1), quite typical of other quiescent neutron stars. Assuming standard core cooling, from the quiescent flux of this source we predict long (> 400 yr) quiescent episodes to allow the neutron star to cool. Alternatively, enhanced core cooling processes are needed to cool down the core. However, if we do not detect the quiescent counterpart of the transient this gives an unabsorbed 0.5-10 keV luminosity upper limit of 8 x 10(31) erg s(-1). We also discuss other X-ray sources within the globular cluster. From the estimated stellar encounter rate of this cluster we find that the number of sources we detect is significantly higher than expected by the relationship of Pooley et al. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. RP Cackett, EM (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM emc14@st-andrews.ac.uk OI Heinke, Craig/0000-0003-3944-6109 NR 56 TC 18 Z9 18 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2006 VL 369 IS 1 BP 407 EP 415 DI 10.1111/j.1365-2966.2006.10315.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046AI UT WOS:000237783400053 ER PT J AU Ross, C Santiago-Vazquez, L Paul, V AF Ross, C Santiago-Vazquez, L Paul, V TI Toxin release in response to oxidative stress and programmed cell death in the cyanobacterium Microcystis aeruginosa SO AQUATIC TOXICOLOGY LA English DT Article DE caspase; cellular stress; hydrogen peroxide; Microcystis aeruginosa; microcystins; programmed cell death ID ULTRAVIOLET-B RADIATION; CHLOROPHYTE DUNALIELLA-TERTIOLECTA; BLUE-GREEN-ALGAE; HYPERSENSITIVE RESPONSE; HYDROGEN-PEROXIDE; DISEASE RESISTANCE; PLANT-CELLS; KEY ROLE; APOPTOSIS; DAMAGE AB An unprecedented bloom of the cyanobacterium, Microcystis aeruginosa Katz. occurred in the St. Lucie Estuary, FL in the summer of 2005. Samples were analyzed for toxicity by ELISA and by use of the polymerase chain reaction (PCR) with specific oligonucleotide primers for the mcyB gene that has previously been correlated with the biosynthesis of toxic microcystins. Despite the fact that secreted toxin levels were relatively low in dense natural assemblages (3.5 mu g l(-1)), detectable toxin levels increased by 90% when M. aeruginosa was stressed by an increase in salinity, physical injury, application of the chemical herbicide paraquat, or UV irradiation. The application of the same stressors caused a three-fold increase in the production of H2O2 when compared to non-stressed cells. The application of micromolar concentrations of H2O2 induced programmed cell death (PCD) as measured by a caspase protease assay. Catalase was capable of inhibiting PCD, implicating H2O2 as the inducing oxidative species. Our results indicate that physical stressors induce oxidative stress, which results in PCD and a concomitant release of toxin into the surrounding media. Remediation strategies that induce cellular stress should be approached with caution since these protocols are capable of releasing elevated levels of microcystins into the environment. (c) 2006 Elsevier B.V. All rights reserved. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Florida Atlantic Univ, Dept Chem & Biochem, Boca Raton, FL 33431 USA. RP Ross, C (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM Ross@sms.si.edu RI Ross, Cliff/B-8291-2011 NR 71 TC 86 Z9 97 U1 2 U2 51 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-445X J9 AQUAT TOXICOL JI Aquat. Toxicol. PD JUN 10 PY 2006 VL 78 IS 1 BP 66 EP 73 DI 10.1016/j.aquatox.2006.02.007 PG 8 WC Marine & Freshwater Biology; Toxicology SC Marine & Freshwater Biology; Toxicology GA 048YV UT WOS:000237983400009 PM 16580745 ER PT J AU Blakeslee, JP Holden, BP Franx, M Rosati, P Bouwens, RJ Demarco, R Ford, HC Homeier, NL Illingworth, GD Jee, MJ Mei, S Menanteau, F Meurer, GR Postman, M Tran, KVH AF Blakeslee, John P. Holden, B. P. Franx, M. Rosati, P. Bouwens, R. J. Demarco, R. Ford, H. C. Homeier, N. L. Illingworth, G. D. Jee, M. J. Mei, S. Menanteau, F. Meurer, G. R. Postman, M. Tran, Kim-Vy H. TI Clusters at half Hubble time: Galaxy structure and colors in RX J0152.7-1357 and MS 1054-03 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : individual (MS 1054-0321, RX J0152.7-1357); galaxies : elliptical and lenticular, cD; galaxies : evolution ID HIGH-REDSHIFT CLUSTER; CHANDRA X-RAY; MORPHOLOGY-DENSITY RELATION; TELESCOPE ADVANCED CAMERA; WEAK-LENSING ANALYSIS; GROTH STRIP SURVEY; SPACE-TELESCOPE; STAR-FORMATION; LUMINOSITY FUNCTION; MAGNITUDE RELATION AB We study the photometric and structural properties of spectroscopically confirmed members in the two massive X-ray-selected z approximate to 0: 83 galaxy clusters MS 1054-03 and RX J0152.7-1357 using three-band mosaic imaging with the Hubble Space Telescope Advanced Camera for Surveys. The samples include 105 and 140 members of RX J0152.7-1357 and MS 1054-03, respectively, to i(775) < 24.0. A quantitative classification scheme using Sersic indices and "bumpiness" (the ratio of the rms residuals to the model mean) was found to correlate well with visual morphological type. The color-magnitude residuals correlate well with the local density, as measured from both galaxy numbers and weak lensing. Weaker correlations are found with cluster radius (the fundamental dependence is on local density). We identify a threshold surface mass density of Sigma approximate to 0: 1, in units of the critical density, above which there are relatively few blue (star-forming) galaxies. In RX J0152.7-1357, there is an offset of 0.006 +/- 0.002 in the mean redshifts of the early- and late-type galaxies, possibly from an infalling foreground association of late-type galaxies. A range of star-formation time-scales are needed to reproduce the galaxy loci in the color-color diagrams. We find rest-frame scatters for the ellipticals of 0.03 +/- 0.01 mag in U - B and 0,07 +/- 0,01 mag in U - V. The mean colors and their scatters imply ages similar to 3.5 Gyr, or formation at z approximate to 2.2. Thus, when the universe was half its present age, cluster ellipticals were about half the age of the universe; the same is coincidentally true of the median ages of ellipticals today. However, the most massive local ellipticals have ages greater than or similar to 10 Gyr, consistent with our results for their likely progenitors at z greater than or similar to 0.8. C1 Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. European So Observ, D-85748 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blakeslee, JP (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. EM jblakes@wsu.edu OI Blakeslee, John/0000-0002-5213-3548 NR 93 TC 100 Z9 100 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 JUN 10 PY 2006 VL 644 IS 1 BP 30 EP 53 DI 10.1086/503539 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200003 ER PT J AU Lai, K Lidz, A Hernquist, L Zaldarriaga, M AF Lai, K Lidz, A Hernquist, L Zaldarriaga, M TI The impact of temperature fluctuations on the Ly alpha forest power spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; intergalactic medium; large-scale structure of universe; quasars : absorption lines ID DIGITAL SKY SURVEY; PHOTOIONIZED INTERGALACTIC MEDIUM; PROBABILITY-DISTRIBUTION FUNCTION; IONIZING-RADIATION FLUCTUATIONS; QUASAR LUMINOSITY FUNCTION; LARGE-SCALE STRUCTURE; QSO REDSHIFT SURVEY; COSMIC REIONIZATION; GALAXY FORMATION; STELLAR SOURCES AB We explore the impact of spatial fluctuations in the intergalactic medium (IGM) temperature on the Ly alpha forest flux power spectrum near z similar to 3. We develop a semianalytic model to examine temperature fluctuations resulting from inhomogeneous H I and incomplete He II reionizations. Detection of these fluctuations might provide insight into the reionization histories of hydrogen and helium. Furthermore, these fluctuations, neglected in previous analyses, could bias constraints on cosmological parameters from the Ly alpha forest. We find that the temperature fluctuations resulting from inhomogeneous H I reionization are likely to be very small, with an rms amplitude of less than or similar to 5%, sigma(T0)/(T-0) less than or similar to 0.05. More important are the temperature fluctuations that arise from incomplete H II reionization, which might plausibly be as large as 50%, sigma(T0)/(T-0) similar to 0.5. In practice, however, these temperature fluctuations have only a small effect on flux power spectrum predictions. The smallness of the effect is possibly due to density fluctuations dominating over temperature fluctuations on the scales probed by current measurements. On the largest scales currently probed, k similar to 0.001 s km(-1) (similar to 0.1 h Mpc(-1)), the effect on the flux power spectrum may be as large as similar to 10% in extreme models. The effect is larger on small scales, up to similar to 20% at k - 0.1 s km(-1), due to thermal broadening. Our results suggest that the omission of temperature fluctuation effects from previous analyses does not significantly bias constraints on cosmological parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Lai, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 68 TC 22 Z9 22 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 61 EP 70 DI 10.1086/503320 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200005 ER PT J AU Martini, P Kelson, DD Kim, E Mulchaey, JS Athey, AA AF Martini, P Kelson, DD Kim, E Mulchaey, JS Athey, AA TI Spectroscopic confirmation of a large population of active galactic nuclei in clusters of galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : clusters : general; galaxies : evolution; X-rays : galaxies; X-rays : galaxies : clusters; X-rays : general ID CHANDRA MULTIWAVELENGTH PROJECT; X-RAY LUMINOSITY; EMISSION-LINE GALAXIES; STAR-FORMATION RATE; RICH CLUSTERS; DISTANT CLUSTERS; POINT SOURCES; COMA CLUSTER; AGN ACTIVITY; CL 1358+62 AB We have completed a spectroscopic survey of X-ray point sources in eight low-redshift clusters of galaxies (0.05 < z < 0.31) and have identified 40 cluster members with broadband (0.3-8 keV) X-ray luminosities between L-X = 8 x 10(40) and 4 x 10(43) ergs s(-1). There are between two and 10 X-ray sources per cluster. We use visible-wavelength emission lines, X-ray spectral shapes, and multiwavelength flux ratios to determine that at least 35 of these galaxies are active galactic nuclei (AGNs). From our spectroscopic survey of other candidate cluster members we estimate that the AGN fraction f(A) is similar to 5% for cluster galaxies more luminous than M-R = -20 mag hosting AGNs with broadband X-ray luminosities above L-X = 10(41) ergs s(-1), or f(A)(M-R < -20; L-X > 10(41)) similar to 5%. We stress that additional, lower luminosity AGNs are expected to be present in the MR < -20 mag cluster members. Our data unambiguously demonstrate that cluster galaxies host AGNs more frequently than previously expected. Only four of these galaxies have obvious visible-wavelength AGN signatures, even though their X-ray luminosities are too high for their X-ray emission to be due to populations of low-mass X-ray binaries or hot, gaseous halos. We attribute the significant difference in visible and X-ray AGN identification to dilution of low-luminosity AGN spectral signatures by host galaxy starlight and/or obscuration of accretion onto the central, supermassive black hole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Pasadena, CA 91101 USA. RP Martini, P (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM martini@astronomy.ohio-state.edu NR 66 TC 82 Z9 82 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 116 EP 132 DI 10.1086/503521 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200010 ER PT J AU Brand, K Dey, A Weedman, D Desai, V Le Floc'h, E Jannuzi, BT Soifer, BT Brown, MJI Eisenhardt, P Gorjian, V Papovich, C Smith, HA Willner, SP Cool, RJ AF Brand, K Dey, A Weedman, D Desai, V Le Floc'h, E Jannuzi, BT Soifer, BT Brown, MJI Eisenhardt, P Gorjian, V Papovich, C Smith, HA Willner, SP Cool, RJ TI The active galactic nuclei contribution to the mid-infrared emission of luminous infrared galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : starburst; infrared : galaxies; X-rays ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; X-RAY SURVEY; 1ST-LOOK SURVEY; SOURCE COUNTS; LOCKMAN HOLE; XBOOTES; DUST; COUNTERPARTS; QUASARS AB We determine the contribution of AGN to the mid-IR emission of luminous infrared galaxies (LIRGs) at z > 0.6 by measuring the mid-IR dust continuum slope of 20,039 mid-IR sources. The 24 mu m sources are selected from a Spitzer MIPS survey of the NOAO Deep Wide-Field Survey Bootes field and have corresponding 8 mu m data from the IRAC Shallow Survey. There is a clear bimodal distribution in the 24 to 8 mu m flux ratio. The X-ray-detected sources fall within the peak corresponding to a flat spectrum in nu f(nu), implying that it is populated by AGN-dominated LIRGs, whereas the peak corresponding to a higher 24 to 8 mu m flux ratio is likely due to LIRGs whose IR emission is powered by starbursts. The 24 mu m emission is increasingly dominated by AGN at higher 24 mu m flux densities (f(24)): the AGN fraction of the z > 0.6 sources increases from 9% at f(24) approximate to 0.35 mJy to 74% +/- 20% at f(24) approximate to 3 mJy, in good agreement with model predictions. Deep 24 mu m, small-area surveys, like GOODS, will be strongly dominated by starburst galaxies. AGN are responsible for similar to 3%-7% of the total 24 mu m background. C1 Natl Opt Astron Observ, Tucson, AZ 85726 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Associated Observ Paris, Galaxies Etoiles Phys & Instrumentat, F-92195 Meudon, France. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brand, K (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85726 USA. EM brand@noao.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 35 TC 81 Z9 81 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 143 EP 147 DI 10.1086/503416 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200012 ER PT J AU Perkins, JS Badran, HM Blaylock, G Bradbury, SM Cogan, P Chow, YCK Cui, W Daniel, MK Falcone, AD Fegan, SJ Finley, JP Fortin, P Fortson, LF Gillanders, GH Gutierrez, KJ Grube, J Hall, J Hanna, D Holder, J Horan, D Hughes, SB Humensky, TB Kenny, GE Kertzman, M Kieda, DB Kildea, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G Moriarty, P Ong, RA Pohl, M Ragan, K Rebillot, PF Sembroski, GH Steele, D Swordy, SP Valcarcel, L Vassiliev, VV Wakely, SP Weekes, TC Williams, DA AF Perkins, JS Badran, HM Blaylock, G Bradbury, SM Cogan, P Chow, YCK Cui, W Daniel, MK Falcone, AD Fegan, SJ Finley, JP Fortin, P Fortson, LF Gillanders, GH Gutierrez, KJ Grube, J Hall, J Hanna, D Holder, J Horan, D Hughes, SB Humensky, TB Kenny, GE Kertzman, M Kieda, DB Kildea, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G Moriarty, P Ong, RA Pohl, M Ragan, K Rebillot, PF Sembroski, GH Steele, D Swordy, SP Valcarcel, L Vassiliev, VV Wakely, SP Weekes, TC Williams, DA CA VERITAS Collaboration TI TeV gamma-ray observations of the Perseus and Abell 2029 galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : individual (NGC 1275); galaxies : clusters : individual (Abell 426, Perseus, Abell 2029); gamma rays : observations ID EXTREME-ULTRAVIOLET EMISSION; VLA SKY SURVEY; COMA CLUSTER; GALACTIC-CENTER; RELIC CANDIDATES; MAGNETIC-FIELDS; RADIO HALO; ORIGIN; TEMPERATURE; RADIATION AB Galaxy clusters might be sources of TeV gamma rays emitted by high-energy protons and electrons accelerated by large-scale structure formation shocks, galactic winds, or active galactic nuclei. Furthermore, gamma rays may be produced in dark matter particle annihilation processes at the cluster cores. We report on observations of the galaxy clusters Perseus and A2029 using the 10 m Whipple Cerenkov telescope during the 2003-2004 and 2004-2005 observing seasons. We apply a two-dimensional analysis technique to scrutinize the clusters for TeV emission. In this paper we first determine flux upper limits on TeVgamma- ray emission from point sources within the clusters. Second, we derive upper limits on the extended cluster emission. We subsequently compare the flux upper limits with EGRET upper limits at 100 MeV and theoretical models. Assuming that the gamma-ray surface brightness profile mimics that of the thermal X-ray emission and that the spectrum of cluster cosmic rays extends all the way from thermal energies to multi-TeV energies with a differential spectral index of similar to 2.1, our results imply that the cosmic-ray proton energy density is less than 7.9% of the thermal energy density for the Perseus Cluster. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Columbia Univ Barnard Coll, Dept Astron, New York, NY 10027 USA. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Perkins, JS (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. RI Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Lang, Mark/0000-0003-4641-4201 NR 48 TC 43 Z9 43 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 148 EP 154 DI 10.1086/503321 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200013 ER PT J AU Machacek, M Jones, C Forman, WR Nulsen, P AF Machacek, M Jones, C Forman, WR Nulsen, P TI Chandra observations of gas stripping in the elliptical galaxy NGC 4552 in the Virgo Cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (Virgo); galaxies : individual (NGC 4552, M89); intergalactic medium; X-rays : galaxies ID X-RAY-EMISSION; INTERSTELLAR-MEDIUM; PERSEUS CLUSTER; S0 GALAXIES; ENVIRONMENT; CATALOG; ROSAT; PARAMETERS; LUMINOSITY; MORPHOLOGY AB We use a 54.4 ks Chandra observation to study ram pressure stripping in NGC 4552 (M89), an elliptical galaxy in the Virgo Cluster. Chandra images in the 0.5-2 keV band show a sharp leading edge in the surface brightness 3.1 kpc north of the galaxy center, a cool (kT = 0.51(-0.06)(+0.09) keV) tail with mean density n(e) similar to (5.4 +/- 1.7) x 10(-3) cm(-3) extending similar to 10 kpc to the south of the galaxy, and two 3-4 kpc horns of emission extending southward away from the leading edge. These are all features characteristic of supersonic ram pressure stripping of galaxy gas, due to NGC 4552's motion through the surrounding Virgo ICM. Fitting the surface brightness profile and spectra across the leading edge, we find the galaxy gas inside the edge is cooler (k(T) = 0.43(-0.02)(+0.03) keV) and denser (n(e) similar to 0.010 cm(-3)) than the surrounding Virgo ICM [kT 2.2(-0.4)(+0.7) keVand n(e) (3.0 +/- 0.3) x 10(-4) cm(-3)]. The resulting pressure ratio between the free-streaming ICM and cluster gas at the stagnation point is similar to 7.6(-2.0)(+3.4) for galaxy gas metallicities of 0.5(-0.3)(+0.5) lZ(circle dot), which suggests that NGC 4552 is moving supersonically through the cluster with a velocity v similar to 1680(-220)(+390) km s(-1) (Mach 2.2(-0.3)(+0.5)) at an angle xi similar to 35 degrees +/- 7 degrees toward us with respect to the plane of the sky. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Machacek, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 NR 72 TC 45 Z9 45 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 155 EP 166 DI 10.1086/503350 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200014 ER PT J AU Morse, JA Smith, N Blair, WP Kirshner, RP Winkler, PF Hughes, JP AF Morse, Jon A. Smith, Nathan Blair, William P. Kirshner, Robert P. Winkler, P. Frank Hughes, John P. TI Hubble Space Telescope observations of oxygen-rich supernova remnants in the Magellanic Clouds. III. WFPC2 imaging of the young, crab-like supernova remnant SNR 0540-69.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : individual (SNR 0540-69.3); Magellanic Clouds; supernova remnants ID CASSIOPEIA-A; CIRCUMSTELLAR RING; SYNCHROTRON NEBULA; OPTICAL-SPECTRUM; FAR-ULTRAVIOLET; PULSAR; SPECTROSCOPY; DISCOVERY; GEOMETRY; NITROGEN AB HST images with WFPC2 of the young, oxygen-rich, Crab-like supernova remnant SNR 0540-69.3 in the Large Magellanic Cloud (LMC) reveal details of the emission distribution and the relationship between the expanding ejecta and synchrotron nebula. The emission distributions appear very similar to those seen in the Crab Nebula, with the ejecta located in a thin envelope surrounding the synchrotron nebula. The [O III] emission is more extended than other tracers, forming a faint "skin" around the denser filaments and synchrotron nebula, as also observed in the Crab. The [O III] exhibits somewhat different kinematic structure in long-slit spectra, including a more extended high-velocity emission halo not seen in images. Yet even the fastest expansion speeds in SNR 0540-69.3's halo are slow when compared to most other young supernova remnants, although the Crab Nebula has similar slow expansion speeds. We show a striking correspondence between the morphology of the synchrotron nebula observed in an optical continuum filter with that recently resolved in Chandra X-ray images. We argue that the multicomponent kinematics and filamentary morphology of the optical emission-line features likely result from magnetic Rayleigh-Taylor instabilities that form as the synchrotron nebula expands and sweeps up ejecta, as seen in the Crab Nebula. Our images and spectra help to refine our understanding of SNR 0540-69.3 in several more detailed respects: they confirm the identification of H alpha + [N II] in the red spectrum, show that the systemic velocity of SNR 0540-69.3 is not significantly different from that of the LMC, and hint at a lower Ne abundance than the Crab (potentially indicating a more massive progenitor star). C1 NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Morse, JA (reprint author), NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Mail Code 665, Greenbelt, MD 20771 USA. EM jon.morse@nasa.gov; nathans@casa.colorado.edu; wpb@pha.jhu.edu; kirshner@cfa.harvard.edu; winkler@panther.middlebury.edu; jph@physics.rutgers.edu NR 38 TC 13 Z9 13 U1 0 U2 2 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 JUN 10 PY 2006 VL 644 IS 1 BP 188 EP 197 DI 10.1086/503313 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200018 ER PT J AU Harvey, PM Chapman, N Lai, SP Evans, NJ Allen, LE Jorgensen, JK Mundy, LG Huard, TL Porras, A Cieza, L Myers, PC Merin, B van Dishoeck, EF Young, KE Spiesman, W Blake, GA Koerner, DW Padgett, DL Sargent, AI Stapelfeldt, KR AF Harvey, Paul M. Chapman, Nicholas Lai, Shih-Ping Evans, Neal J., II Allen, Lori E. Jorgensen, Jes K. Mundy, Lee G. Huard, Tracy L. Porras, Alicia Cieza, Lucas Myers, Philip C. Merin, Bruno van Dishoeck, Ewine F. Young, Kaisa E. Spiesman, William Blake, Geoffrey A. Koerner, David W. Padgett, Deborah L. Sargent, Anneila I. Stapelfeldt, Karl R. TI The Spitzer c2d survey of large, nearby, insterstellar clouds. II. Serpens observed with IRAC SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : ISM; ISM : clouds ID YOUNG STELLAR OBJECTS; HERBIG AE/BE STARS; LARGE-MAGELLANIC-CLOUD; MAIN-SEQUENCE STARS; MOLECULAR CLOUD; INFRARED OBSERVATIONS; OPHIUCHI CLOUD; CORE; EMISSION; MICRON AB We present maps of 0.89 deg(2) of the Serpens dark cloud at 3.6, 4.5, 5.8, and 8.0 mu m observed with the Spitzer Space Telescope Infrared Array Camera (IRAC). We discuss in detail the data processing carried out by the c2d team on IRAC data. More than 100,000 compact sources have been extracted, but we confine most of our discussion to the most reliable subset of these sources. This includes those that are detected above 7 sigma in all four IRAC bands or those detected in the two shorter IRAC bands together with 2MASS. We estimate completeness limits for our survey from Monte Carlo tests with artificial sources inserted into the Spitzer maps. We compare source counts, colors, and magnitudes in the Serpens cloud to two reference data sets, a 0.10 deg(2) set of low-extinction regions near the dark cloud and a 1 deg(2) subset of the SWIRE Elais N1 data that was processed through our pipeline. We find that it is possible to identify more than 200 young stellar object (YSO) candidates from color-magnitude and color-color diagrams, most of which were previously unknown. In addition to the dense area of new star formation known before in the "core'' region ( cluster A), we also find a moderately rich area to the south ( cluster B). Our mapped area also includes the Herbig Ae star VV Ser, whose Spitzer images have been carefully modeled in a separate study. The extreme sensitivity of Spitzer IRAC allows us to search to very low luminosity limits for young substellar objects. The comparison of the Serpens region with the reference areas suggests that a population of infrared excess sources exists in Serpens at least down to luminosities of L similar to 10(-3) L(.) and possibly lower. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Harvey, PM (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM pmh@astro.as.utexas.edu; chapman@astro.umd.edu; slai@astro.umd.edu; nje@astro.as.utexas.edu; leallen@cfa.harvard.edu; jjorgensen@cfa.harvard.edu; lgm@astro.umd.edu; thuard@cfa.harvard.edu; aporras@cfa.harvard.edu; lcieza@astro.as.utexas.edu; pmyers@cfa.harvard.edu; merin@strw.leidenuniv.nl; ewin@strw.leidenuniv.nl; kaisa@astro.as.utexas.edu; spies@astro.as.utexas.edu; gab@gps.caltech.edu; koerner@physics.nau.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu; krs@exoplanet.jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012 NR 46 TC 115 Z9 115 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 JUN 10 PY 2006 VL 644 IS 1 BP 307 EP 325 DI 10.1086/503520 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200027 ER PT J AU Young, KE Enoch, ML Evans, NJ Glenn, J Sargent, A Huard, TL Aguirre, J Golwala, S Haig, D Harvey, P Laurent, G Mauskopf, P Sayers, J AF Young, Kaisa E. Enoch, Melissa L. Evans, Neal J., II Glenn, Jason Sargent, Anneila Huard, Tracy L. Aguirre, James Golwala, Sunil Haig, Douglas Harvey, Paul Laurent, Glenn Mauskopf, Philip Sayers, Jack TI Bolocam survey for 1.1 mm dust continuum emission in the c2d legacy clouds. II. Ophiuchus SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : individual (Ophiuchus molecular cloud); submillimeter ID INITIAL MASS FUNCTION; STAR-FORMATION; LUMINOSITY FUNCTION; MOLECULAR CLOUDS; SOLAR NEIGHBORHOOD; STELLAR; CORES; PROTOSTARS; PERSEUS; REGIONS AB We present a large-scale millimeter continuum map of the Ophiuchus molecular cloud. Nearly 11 deg(2), including all of the area in the cloud with A(V) >= 3 mag, was mapped at 1.1 mm with Bolocam on the Caltech Submillimeter Observatory (CSO). By design, the map also covers the region mapped in the infrared with the Spitzer Space Telescope. We detect 44 definite sources, and a few likely sources are also seen along a filament in the eastern streamer. The map indicates that dense cores in Ophiuchus are very clustered and often found in filaments within the cloud. Most sources are round, as measured at the half-power point, but elongated when measured at lower contour levels, suggesting spherical sources lying within filaments. The masses, for an assumed dust temperature of 10 K, range from 0.24 to 3.9 M(.), with a mean value of 0.96 M(.). The total mass in distinct cores is 42 M(.), 0.5% - 2% of the total cloud mass, and the total mass above 4 sigma is about 80 M(.). The mean densities in the cores are quite high, with an average of 1.6x 10(6) cm(-3), suggesting short free-fall times. The core mass distribution can be fitted with a power law with slope alpha = 2.1 +/- 0.3 for M > 0.5 M(.), similar to that found in other regions, but slightly shallower than that of some determinations of the local IMF. In agreement with previous studies, our survey shows that dense cores account for a very small fraction of the cloud volume and total mass. They are nearly all confined to regions with A(V) >= 9 mag, a lower threshold than found previously. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Cardiff Univ, Cardiff CF24 3YB, Wales. RP Young, KE (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM kaisa@astro.as.utexas.edu; menoch@astro.caltech.edu; nje@astro.as.utexas.edu; jason.glenn@colorado.edu; afs@phobos.caltech.edu; thuard@cfa.harvard.edu; james.aguirre@Colorado.edu; golwala@phobos.caltech.edu; douglas.haig@astro.cf.ac.uk; pmh@astro.as.utexas.edu; glenn.laurent@colorado.edu; philip.mauskopf@astro.cf.ac.uk; jack@its.caltech.edu NR 45 TC 72 Z9 73 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 JUN 10 PY 2006 VL 644 IS 1 BP 326 EP 343 DI 10.1086/503327 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200028 ER PT J AU Zurita, C Torres, MAP Steeghs, D Rodriguez-Gil, P Munoz-Darias, T Casares, J Shahbaz, T Martinez-Pais, IG Zhao, P Garcia, MR Piccioni, A Bartolini, C Guarnieri, A Bloom, JS Blake, CH Falco, EE Szentgyorgyi, A Skrutskie, M AF Zurita, C Torres, MAP Steeghs, D Rodriguez-Gil, P Munoz-Darias, T Casares, J Shahbaz, T Martinez-Pais, IG Zhao, P Garcia, MR Piccioni, A Bartolini, C Guarnieri, A Bloom, JS Blake, CH Falco, EE Szentgyorgyi, A Skrutskie, M TI The 2005 outburst of the halo black hole X-ray transient XTE J1118+480 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (XTE J1118+480, KVUMa); X-rays : stars ID NOVA XTE J1118+480; MULTIWAVELENGTH OBSERVATIONS; OPTICAL COUNTERPART; ACCRETION DISK; GRO JO422+32; LIGHT CURVES; JET MODEL; QUIESCENCE; SPECTRUM; STATE AB We present optical and infrared monitoring of the 2005 outburst of the halo black hole X-ray transient XTE J1118+480. We measured a total outburst amplitude of similar to 5.7 +/- 0.1 mag in the R band and similar to 5 mag in the infrared J, H, and K-s bands. The hardness ratio HR2 (5-12 keV : 3-5 keV) from the RXTE ASM data is 1.53 +/- 0.02 at the peak of the outburst, indicating a hard spectrum. Both the shape of the light curve and the ratio L-X(1-10 keV)/ L-opt resemble the minioutbursts observed in GROJ0422+32 and XTE J1859+226. During early decline, we find a 0.02 mag amplitude variation consistent with a superhump modulation, like the one observed during the 2000 outburst. Similarly, XTE J1118+480 displayed a double-humped ellipsoidal modulation distorted by a superhump wave when settled into a near-quiescence level, suggesting that the disk expanded to the 3: 1 resonance radius after outburst, where it remained until early quiescence. The system reached quiescence at R = 19.02 +/- 0.03, about 3 months after the onset of the outburst. The optical rise preceded the X-ray rise by at most 4 days. The spectral energy distributions (SEDs) at the different epochs during outburst are all quasi - power laws with F-nu proportional to nu(alpha) increasing toward the blue. At the peak of the outburst, we derived alpha = 0.49 +/- 0.04 for the optical data alone and alpha = 0.1 +/- 0.1 when fitting solely the infrared. This difference between the optical and the infrared SEDs suggests that the infrared is dominated by a different component ( a jet?), whereas the optical is presumably showing the disk evolution. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. Univ Bologna, Dipartimento Astron, Bologna, Italy. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Zurita, C (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. EM czurita@iac.es RI Steeghs, Danny/C-5468-2009; Rodriguez-Gil, Pablo/H-7709-2015 OI Steeghs, Danny/0000-0003-0771-4746; Rodriguez-Gil, Pablo/0000-0002-4717-5102 NR 53 TC 21 Z9 21 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 432 EP 438 DI 10.1086/503286 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200037 ER PT J AU Winn, JN Hamilton, CM Herbst, WJ Hoffman, JL Holman, MJ Johnson, JA Kuchner, MJ AF Winn, JN Hamilton, CM Herbst, WJ Hoffman, JL Holman, MJ Johnson, JA Kuchner, MJ TI The orbit and occultations of KH 15D SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations : individual (NGC 2264) stars : individual (KH 15D); stars : pre-main-sequence ID T-TAURI STARS; LOW-MASS STARS; NGC 2264; MYSTERIOUS ECLIPSES; LIGHT CURVES; SYSTEM; BINARY; SPECTROSCOPY; PHOTOMETRY; EMISSION AB The unusual flux variations of the pre-main-sequence binary star KH 15D have been attributed to occultations by a circumbinary disk. We test whether or not this theory is compatible with newly available data, including recent radial velocity measurements, CCD photometry over the past decade, and photographic photometry over the past 50 years. We find the model to be successful, after two refinements: a more realistic motion of the occulting feature and a halo around each star that probably represents scattering by the disk. The occulting feature is exceptionally sharp edged, raising the possibility that the dust in the disk has settled into a thin layer and providing a tool for fine-scale mapping of the immediate environment of a T Tauri star. However, the window of opportunity is closing, as the currently visible star may be hidden at all orbital phases by as early as 2008. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. Univ Massachusetts, Five Coll Astron Dept, Amherst, MA 01003 USA. Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Winn, JN (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Kuchner, Marc/E-2288-2012 NR 49 TC 30 Z9 31 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 510 EP 524 DI 10.1086/503417 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200045 ER PT J AU Turnbull, MC Traub, WA Jucks, KW Woolf, NJ Meyer, MR Gorlova, N Skrutskie, MF Wilson, JC AF Turnbull, MC Traub, WA Jucks, KW Woolf, NJ Meyer, MR Gorlova, N Skrutskie, MF Wilson, JC TI Spectrum of a habitable world: Earthshine in the near-infrared SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; Moon; planetary systems ID EXTRASOLAR TERRESTRIAL PLANETS; CLOUDS; SATELLITES; SURFACES; DISK; ICE AB To characterize the spectrum of Earth viewed as an extrasolar planet, we observed the spatially integrated near-infrared (0.7 - 2.4 mu m) reflection spectrum of Earth via the dark side of the Moon (earthshine). After contributions from the Sun, Moon, and local atmosphere were removed, the resulting spectrum was fitted with a simple model of the reflectivity of Earth. The best model fit is dominated by the reflection spectrum of the atmosphere above medium-altitude water clouds, with lesser contributions from high-altitude ice clouds and from the ground. The spectral features seen are H2O ( six strong band structures from 0.7 to 2.0 mu m), CO2 (six moderate-strength features from 1.4 to 2.1 mu m), O-2 (two moderate-strength features at 0.76 and 1.26 mu m), and several weak CH4 features. Interpreted as a spectrum of an extrasolar planet, we would confidently conclude that this is a habitable planet, based on the presence of strong water bands. Furthermore, the simultaneous presence of oxygen and methane is a strong indicator of biological activity. We might also conclude that the planet is geologically active, based on the presence of CO2, water, and a dynamic atmosphere ( inferred from cirrus clouds, cumulus clouds, and clear-air fractions in our model fit). This suggests that it would be valuable for the Terrestrial Planet Finder - Coronagraph (TPF-C) mission to include near-infrared spectroscopy capability. On the basis of the present work, we suggest that future long-term monitoring of the earthshine would allow us to discern how the globally integrated spectrum changes with planet rotation, cloud cover, and seasons. C1 Carnegie Inst Washington, Washington, DC 20008 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Turnbull, MC (reprint author), Carnegie Inst Washington, 5241 Broad Branch Rd, Washington, DC 20008 USA. EM turnbull@dtm.ciw.edu; wtraub@jpl.nasa.gov NR 27 TC 68 Z9 68 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2006 VL 644 IS 1 BP 551 EP 559 DI 10.1086/503322 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XK UT WOS:000238339200048 ER PT J AU Gould, A Udalski, A An, D Bennett, DP Zhou, AY Dong, S Rattenbury, NJ Gaudi, BS Yock, PCM Bond, IA Christie, GW Horne, K Anderson, J Stanek, KZ Depoy, DL Han, C McCormick, J Park, BG Pogge, RW Poindexter, SD Soszynski, I Szymanski, MK Kubiak, M Pietrzynski, G Szewczyk, O Wyrzykowski, L Ulaczyk, K Paczynski, B Bramich, DM Snodgrass, C Steele, IA Burgdorf, MJ Bode, MF Botzler, CS Mao, S Swaving, SC AF Gould, A. Udalski, A. An, D. Bennett, D. P. Zhou, A. -Y. Dong, S. Rattenbury, N. J. Gaudi, B. S. Yock, P. C. M. Bond, I. A. Christie, G. W. Horne, K. Anderson, J. Stanek, K. Z. DePoy, D. L. Han, C. McCormick, J. Park, B. -G. Pogge, R. W. Poindexter, S. D. Soszynski, I. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Szewczyk, O. Wyrzykowski, L. Ulaczyk, K. Paczynski, B. Bramich, D. M. Snodgrass, C. Steele, I. A. Burgdorf, M. J. Bode, M. F. Botzler, C. S. Mao, S. Swaving, S. C. TI Microlens OGLE-2005-BLG-169 implies that cool Neptune-like planets are common SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : bulge; gravitational lensing; planetary systems ID HIGH-MAGNIFICATION; IMAGE SUBTRACTION; EXTRASOLAR PLANETS; GALACTIC BULGE; SYSTEMS; COMPANIONS; PHOTOMETRY; EVENTS; MASSES; MODEL AB We detect a Neptune mass ratio (similar or equal to 8 x 10(-5)) planetary companion to the lens star in the extremely high magnification (A similar to 800) microlensing event OGLE-2005-BLG-169. If the parent is a main-sequence star, it has mass M similar to 0.5 M(circle dot), implying a planet mass of similar to 13 M(circle plus) and projected separation of similar to 2.7 AU. When intensely monitored over their peak, high-magnification events similar to OGLE-2005-BLG-169 have nearly complete sensitivity to Neptune mass ratio planets with projected separations of 0.6-1.6 Einstein radii, corresponding to 1.6-4.3 AU in the present case. Only two other such events were monitored well enough to detect Neptunes, and so this detection by itself suggests that Neptune mass ratio planets are common. Moreover, another Neptune was recently discovered at a similar distance from its parent star in a low-magnification event, which are more common but are individually much less sensitive to planets. Combining the two detections yields 90% upper and lower frequency limits f = 0.38(-0.22)(+0.31) over just 0.4 decades of planet- star separation. In particular, f > 16% at 90% confidence. The parent star hosts no Jupitermass companions with projected separations within a factor 5 of that of the detected planet. The lens-source relative proper motion is mu similar to 7-10 mas yr(-1), implying that if the lens is sufficiently bright, I less than or similar to 23.8, it will be detectable by the Hubble Space Telescope by 3 years after peak. This would permit a more precise estimate of the lens mass and distance and, so, the mass and projected separation of the planet. Analogs of OGLE-2005-BLG-169Lb orbiting nearby stars would be difficult to detect by other methods of planet detection, including radial velocities, transits, and astrometry. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Uniwersytetu Warszawskiego, Astron Observ, PL-00478 Warsaw, Poland. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Auckland, Dept Phys, Auckland 1001, New Zealand. Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand. Auckland Observ, Auckland, New Zealand. Univ St Andrews, Scottish Univ Phys Alliance, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Farm Cove Observ, Ctr Backyard Astrophys, Auckland 1706, New Zealand. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. Univ Concepcion, Dept Fis, Concepcion, Chile. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Princeton Univ Observ, Princeton, NJ 08544 USA. Queens Univ Belfast, Dept Phys & Astron, Astrophys Res Inst, Belfast BT7 1NN, Antrim, North Ireland. RP Gould, A (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM gould@astronomy.ohio-state.edu; udalski@astrouw.edu.pl RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Bennett, David/O-2136-2013; OI Bennett, David/0000-0001-8043-8413; Snodgrass, Colin/0000-0001-9328-2905 NR 27 TC 194 Z9 194 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 JUN 10 PY 2006 VL 644 IS 1 BP L37 EP L40 DI 10.1086/505421 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XM UT WOS:000238339400010 ER PT J AU Carter, LM Campbell, DB Campbell, BA AF Carter, LM Campbell, DB Campbell, BA TI Volcanic deposits in shield fields and highland regions on Venus: Surface properties from radar polarimetry SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ELECTRICAL-PROPERTIES; MAGELLAN; ROUGHNESS; EMISSION; ARECIBO AB [1] We compare Arecibo dual-polarization radar image data for Venus to Magellan images and emissivity data to investigate the physical properties of volcanic deposits. Radar waves can easily penetrate smooth mantling layers such as ash, aeolian and crater-derived deposits. If a circularly polarized radar wave refracts into a surface that is smooth at wavelength scales, the vertical component of the wave will be preferentially transmitted, resulting in a net linear-polarized echo component. Arecibo polarimetry data were used to create maps of the degree of linear polarization in the radar echo. We find that some volcanic fields in plains regions on Venus are associated with enhanced linear polarization. These fields sometimes have nearby windstreaks which suggest fine-grained surface material, and we infer that the radar wave is penetrating into mantling deposits that are a few centimeters to similar to 1 m thick. Enhanced linear polarization values are also correlated with specific lava flows. These lava flows have emissivity values of 0.80 to 0.84, similar to many other flows on Venus. The enhanced linear polarization may be produced by penetration of the radar wave into very smooth lava flows with internal air gaps. High-reflectivity, low-emissivity areas near the summits of Theia and Tepev Montes also have a linearly polarized echo component consistent with surface penetration by the radar wave. The cause of the high linear polarization in summit regions remains uncertain, but perhaps the radar wave is able to penetrate into high dielectric material in limited cases of very smooth surface texture. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Carter, LM (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, POB 37012, Washington, DC 20013 USA. EM carterl@si.edu RI Carter, Lynn/D-2937-2012 NR 28 TC 12 Z9 12 U1 2 U2 5 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 JUN 10 PY 2006 VL 111 IS E6 AR E06005 DI 10.1029/2005JE002519 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 052GL UT WOS:000238220600002 ER PT J AU Miura, O Kuris, AM Torchin, ME Hechinger, RF Chiba, S AF Miura, Osamu Kuris, Armand M. Torchin, Mark E. Hechinger, Ryan F. Chiba, Satoshi TI Parasites alter host phenotype and may create a new ecological niche for snail hosts SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE parasite; host; gigantism; behavioural modification; stable carbon isotope ratio ID CERITHIDEA-CALIFORNICA; INTERMEDIATE HOST; LIFE-HISTORY; BEHAVIOR; POPULATIONS; CASTRATION; GROWTH; TREMATODA; FISH AB By modifying the behaviour and morphology of hosts, parasites may strongly impact host individuals, populations and communities. We examined the effects of a common trematode parasite on its snail host, Batillaria cumingi (Batillariidae). This widespread snail is usually the most abundant invertebrate in salt marshes and mudflats of the northeastern coast of Asia. More than half (52.6%, n = 1360) of the snails in our study were infected. We found that snails living in the lower intertidal zone were markedly larger and exhibited different shell morphology than those in the upper intertidal zone. The large morphotypes in the lower tidal zone were all infected by the trematode, Cercaria batillariae (Heterophyidae). We used a transplant experiment, a mark-and-recapture experiment and stable carbon isotope ratios to reveal that snails infected by the trematode move to the lower intertidal zone, resume growth after maturation and consume different resources. By simultaneously changing the morphology and behaviour of individual hosts, this parasite alters the demographics and potentially modifies resource use of the snail population. Since trematodes are common and often abundant in marine and freshwater habitats throughout the world, their effects potentially alter food webs in many systems. C1 Tohoku Univ, Grad Sch Life Sci, Dept Ecol & Evolutionary Biol, Sendai, Miyagi 9808578, Japan. Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Miura, O (reprint author), Tohoku Univ, Grad Sch Life Sci, Dept Ecol & Evolutionary Biol, Sendai, Miyagi 9808578, Japan. EM 3-ura@biology.tohoku.ac.jp RI Hechinger, Ryan/F-6754-2010 NR 41 TC 57 Z9 59 U1 8 U2 47 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUN 7 PY 2006 VL 273 IS 1592 BP 1323 EP 1328 DI 10.1098/rspb.2005.3451 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 045ZB UT WOS:000237780100003 PM 16777719 ER PT J AU Kharchenko, V Dalgarno, A Schultz, DR Stancil, PC AF Kharchenko, V. Dalgarno, A. Schultz, D. R. Stancil, P. C. TI Ion emission spectra in the Jovian X-ray aurora SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ENERGETIC OXYGEN; JUPITER; PRECIPITATION; MAGNETOSPHERE; ATMOSPHERE AB X-ray and Extreme Ultraviolet emission spectra resulting from energetic sulfur and oxygen ions precipitating into the Jovian atmosphere are calculated. Monte Carlo simulations of the energy and charge relaxation of downward ion fluxes are carried out, using updated collision cross sections for stripping, electron capture, and target ionization. Energy and charge distributions of precipitating sulfur ions are presented for the first time and the equilibrium charge model is shown to be inadequate. X-ray emission spectra are calculated for different sulfur and oxygen mixtures and for different initial entry energies. Satisfactory agreement with both Chandra and XMM-Newton observations is obtained by an equal population of sulfur and oxygen ions with energies between 1 and 2 MeV/amu. The agreement provides a reconciliation of the two spectral data sets and the inferred initial energies are consistent with the view that the ions are magnetospheric in origin and have been accelerated to MeV/amu energies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vkharchenko@cfa.harvard.edu NR 18 TC 30 Z9 30 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 6 PY 2006 VL 33 IS 11 AR L11105 DI 10.1029/2006GL026039 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 052FN UT WOS:000238217800004 ER PT J AU Lowenstein, JM Reuther, JD Hood, DG Scheuenstuhl, G Gerlach, SC Ubelaker, DH AF Lowenstein, JM Reuther, JD Hood, DG Scheuenstuhl, G Gerlach, SC Ubelaker, DH TI Identification of animal species by protein radioimmunoassay of bone fragments and bloodstained stone tools SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE forensic science; archaeology; radioimmunoassay; bone fragments; bloodstains; species identification ID BLOOD RESIDUES; ARTIFACTS AB In forensics and archaeology, it is important to distinguish human from animal remains and to identify animal species from fragmentary bones and bloodstains. We report blind tests in which a protein radioimmunoassay (ARIA) was used to identify the species of six bone fragments lacking morphological specificity and 43 bloodstained lithic tools, knapped experimentally and soaked in blood of known animal and human origin. The submitters of the bone fragments and the bloodstained tools each listed a number of possible species, from which the testers selected the best match with the pRIA results. All six bone fragments were correctly identified: three humans, a deer, a dog, and a cow. Forty-three tools were stained with blood from a wide variety of species including ungulates, carnivores, a fish, and a bird. On 40 of these 43, at least one species (or blood-free control) was identified correctly. Some of the tools were stained with blood of two different species. A mixture of sheep and musk ox blood was correctly identified; in several other mixtures, only a single species was detected. Two tools with human blood and one with human sweat were correctly reported as human. There was a single false positive (one of three controls reported as weakly bovine) and no false negatives. We conclude that the pRIA technique shows a high degree of accuracy in discriminating human from animal bone fragments and bloodstains and in identifying animal species. (c) 2005 Elsevier Ireland Ltd. All rights reserved. C1 Calif Pacific Med Ctr, Dept Nucl Med, San Francisco, CA 94115 USA. No Land Use Res Inc, Fairbanks, AK 99709 USA. MicroAnalyt LLC, Miami, FL USA. Univ Alaska, Dept Anthropol, Fairbanks, AK USA. MRC, NMNH, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Lowenstein, JM (reprint author), Calif Pacific Med Ctr, Dept Nucl Med, 2333 Buchanan St, San Francisco, CA 94115 USA. EM jlowen@itsa.ucsf.edu NR 14 TC 19 Z9 21 U1 1 U2 11 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD JUN 2 PY 2006 VL 159 IS 2-3 BP 182 EP 188 DI 10.1016/j.forsciint.2005.08.007 PG 7 WC Medicine, Legal SC Legal Medicine GA 052WP UT WOS:000238264900014 PM 16191470 ER PT J AU Nakajima, H Sugita, T Irie, H Saitoh, N Kanzawa, H Oelhaf, H Wetzel, G Toon, GC Sen, B Blavier, JF Traub, WA Jucks, K Johnson, DG Yokota, T Sasano, Y AF Nakajima, H. Sugita, T. Irie, H. Saitoh, N. Kanzawa, H. Oelhaf, H. Wetzel, G. Toon, G. C. Sen, B. Blavier, J. -F. Traub, W. A. Jucks, K. Johnson, D. G. Yokota, T. Sasano, Y. TI Measurements of ClONO2 by the Improved Limb Atmospheric Spectrometer (ILAS) in high-latitude stratosphere: New products using version 6.1 data processing algorithm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NITRIC-ACID TRIHYDRATE; ARCTIC VORTEX; SPECTROSCOPIC DATABASE; RETRIEVAL ALGORITHM; OPTICAL-CONSTANTS; CHLORINE NITRATE; OZONE DEPLETION; POLAR VORTEX; VALIDATION; PROFILES AB We report the first continuous measurements of chlorine nitrate (ClONO2) in high-latitude regions taken by the Improved Limb Atmospheric Spectrometer (ILAS) on board the Advanced Earth Observing Satellite (ADEOS) and processed using the latest data retrieval algorithm (version 6.1). Performance of the measurements, validation with three balloon-borne sensors, and seasonal variation of ClONO2 in the Arctic and Antarctic stratosphere are presented, as well as a brief description of the version 6.1 algorithm and data characteristics for both the Arctic and Antarctic. Although the ILAS-measured ClONO2 data show, on average, similar to 30% lower values than the validation data, they agree with validation data within the combined total error (similar to 20-40%) of the ClONO2 measurements at similar to 15- to 32-km altitudes. In the Arctic, enhancement of ClONO2 amounts was observed in spring 1997 after the appearance of polar stratospheric clouds (PSCs) inside the polar vortex. This is the result of preference for ClONO2 formation rather than HCl after the activation of ClOx in this Arctic spring of 1997. In the Antarctic, ClONO2 amounts showed strong local time/latitudinal dependence around the austral fall equinox in 1997. C1 Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. Japan Agcy Marine Earth Sci & Technol, Frontier Res Ctr Global Change, Yokohama, Kanagawa 2360001, Japan. Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan. Forschungszentrum Karlsruhe, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Nakajima, H (reprint author), Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. EM hide@nies.go.jp RI Sasano, Yasuhiro/C-2927-2009; Wetzel, Gerald/A-7065-2013; Oelhaf, Hermann/A-7895-2013; Johnson, David/F-2376-2015; OI Sasano, Yasuhiro/0000-0001-7470-5642; Johnson, David/0000-0003-4399-5653; Sugita, Takafumi/0000-0002-0508-7040 NR 51 TC 12 Z9 12 U1 0 U2 0 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 JUN 2 PY 2006 VL 111 IS D11 AR D11S09 DI 10.1029/2005JD006441 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 050ES UT WOS:000238070900003 ER PT J AU Laube, S Zotz, G AF Laube, Stefan Zotz, Gerhard TI Neither host-specific nor random: Vascular epiphytes on three tree species in a Panamanian lowland forest SO ANNALS OF BOTANY LA English DT Article DE epiphytes; community assembly; null model; host preference; colonization; Panama; Orchidaceae; Bromeliaceae; Araceae ID POPULATION-DYNAMICS; TROPICAL FOREST; WATER RELATIONS; RAIN-FOREST; BIOGEOGRAPHY; DIVERSITY; HABITAT; GROWTH; CAM AB Background and Aims A possible role of host tree identity in the structuring of vascular epiphyte communities has attracted scientific attention for decades. Specifically, it has been suggested that each host tree species has a specific subset of the local species pool according to its own set of properties, e.g. physicochemical characteristics of the bark, tree architecture, or leaf phenology patterns. Methods A novel, quantitative approach to this question is presented, taking advantage of a complete census of the vascular epiphyte community in 0.4 ha of undisturbed lowland forest in Panama. For three locally common host-tree species (Socratea exorrhiza, Marila laxiflora, Perebea xanthochyma) null models were created of the expected epiphyte assemblages assuming that epiphyte colonization reflected random distribution of epiphytes in the forest. Key Results In all three tree species, abundances of the majority of epiphyte species (69-81 %) were indistinguishable from random, while the remaining species were about equally over- or under-represented compared with their occurrence in the entire forest plot. Permutations based on the number of colonized trees (reflecting observed spatial patchiness) yielded similar results. Finally, a third analysis (canonical correspondence analysis) also confirmed host-specific differences in epiphyte assemblages. In spite of pronounced preferences of some epiphytes for particular host trees, no epiphyte species was restricted to a single host. Conclusions The epiphytes on a given tree species are not simply a random sample of the local species pool, but there are no indications of host specificity either. C1 Fachbereich Biol, Abt Pflanzenbiol & Syst 13274, D-67653 Kaiserslautern, Germany. Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Laube, S (reprint author), Fachbereich Biol, Abt Pflanzenbiol & Syst 13274, D-67653 Kaiserslautern, Germany. EM s.laube@web.de NR 39 TC 54 Z9 61 U1 1 U2 13 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 JUN PY 2006 VL 97 IS 6 BP 1103 EP 1114 DI 10.1093/aob/mc1067 PG 12 WC Plant Sciences SC Plant Sciences GA 060QN UT WOS:000238816800019 PM 16574691 ER PT J AU Jiang, LH Fan, XH Cool, RJ Eisenstein, DJ Zehavi, I Richards, GT Scranton, R Johnston, D Strauss, MA Schneider, DP Brinkmann, J AF Jiang, LH Fan, XH Cool, RJ Eisenstein, DJ Zehavi, I Richards, GT Scranton, R Johnston, D Strauss, MA Schneider, DP Brinkmann, J TI A spectroscopic survey of faint quasars in the SDSS deep stripe. I. Preliminary results from the co-added catalog SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : luminosity function, mass function; quasars : general; surveys ID DIGITAL-SKY-SURVEY; HIGH-REDSHIFT QUASARS; SURVEY COMMISSIONING DATA; OPTICAL LUMINOSITY FUNCTION; FALL EQUATORIAL STRIPE; ACTIVE GALACTIC NUCLEI; DATA RELEASE; TARGET SELECTION; BLACK-HOLES; STELLAR OBJECTS AB In this paper we present the first results of a deep spectroscopic survey of faint quasars in the Sloan Digital Sky Survey (SDSS) Southern Survey, a deep survey carried out by repeatedly imaging a 270 deg(2) area. Quasar candidates were selected from the deep data with good completeness over 0 < z < 5 and 2-3 mag fainter than the SDSS main survey. Spectroscopic follow-up was carried out on the 6.5 mMMT with Hectospec. The preliminary sample of this SDSS faint quasar survey (SFQS) covers similar to 3.9 deg(2), contains 414 quasars, and reaches g=22.5. The overall selection efficiency is similar to 66% (similar to 80% at g < 21.5); the efficiency in the most difficult redshift range (2 < z < 3) is better than 40%. We use the 1/V-a method to derive a binned estimate of the quasar luminosity function (QLF) and model the QLF using maximum likelihood analysis. The best model fits confirm previous results showing that the QLF has steep slopes at the bright end and much flatter slopes (-1.25 at z less than or similar to 2.0 and similar to 1.55 at z greater than or similar to 2: 0) at the faint end, indicating a break in the QLF slope. Using a luminosity-dependent density evolution model, we find that the quasar density at M-g < -22.5 peaks at z similar to 2, which is later in cosmic time than the peak of z similar to 2.5 found from surveys of more luminous objects. The SFQS QLF is consistent with the results of the 2dF QSO Redshift Survey, the SDSS, and the 2dF-SDSS LRG and QSO Survey, but probes fainter quasars. We plan to obtain more quasars from future observations and establish a complete faint quasar sample with more than 1000 objects over 10 deg2. C1 Smithsonian Inst, MMT Observ, Washington, DC 20560 USA. Univ Arizona, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Apache Point Observ, Sunspot, NM 88349 USA. RP Jiang, LH (reprint author), Smithsonian Inst, MMT Observ, Washington, DC 20560 USA. RI Jiang, Linhua/H-5485-2016 OI Jiang, Linhua/0000-0003-4176-6486 NR 72 TC 58 Z9 58 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2006 VL 131 IS 6 BP 2788 EP 2800 DI 10.1086/503745 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 051QT UT WOS:000238176400004 ER PT J AU Ridge, NA Di Francesco, J Kirk, H Li, D Goodman, AA Alves, JF Arce, HG Borkin, MA Caselli, P Foster, JB Heyer, MH Johnstone, D Kosslyn, DA Lombardi, M Pineda, JE Schnee, SL Tafalla, M AF Ridge, NA Di Francesco, J Kirk, H Li, D Goodman, AA Alves, JF Arce, HG Borkin, MA Caselli, P Foster, JB Heyer, MH Johnstone, D Kosslyn, DA Lombardi, M Pineda, JE Schnee, SL Tafalla, M TI The COMPLETE Survey of Star-Forming Regions: Phase I data SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : clouds; stars : formation; surveys ID DARK CLOUD COMPLEX; INTERSTELLAR EXTINCTION; MAGNETIC-FIELD; EMISSION MAPS; PERSEUS; DUST; DENSITY; MICRONS AB We present an overview of data available for the Ophiuchus and Perseus molecular clouds from Phase I of the COMPLETE Survey of Star-Forming Regions. This survey provides a range of data complementary to the Spitzer Legacy Program "From Molecular Cores to Planet Forming Disks.'' Phase I includes the following: extinction maps derived from the Two Micron All Sky Survey (2MASS) near-infrared data using the NICER algorithm; extinction and temperature maps derived from IRAS 60 and 100 mu m emission; H I maps of atomic gas; (CO)-C-12 and (CO)-C-13 maps of molecular gas; and submillimeter continuum images of emission from dust in dense cores. Not unexpectedly, the morphology of the regions appears quite different depending on the column density tracer that is used, with IRAS tracing mainly warmer dust and CO being biased by chemical, excitation, and optical depth effects. Histograms of column density distribution are presented, showing that extinction as derived from 2MASS NICER gives the closest match to a lognormal distribution, as is predicted by numerical simulations. All the data presented in this paper, and links to more detailed publications on their implications, are publicly available at the COMPLETE Web site. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Herzberg Inst Astrophys, Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. European So Observ, D-85748 Garching, Germany. Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Massachusetts, Dept Astron, Lederle Grad Res Ctr, Amherst, MA 01003 USA. Observ Astron Nacl, E-28014 Madrid, Spain. RP Ridge, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010; OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477; Johnstone, Doug/0000-0002-6773-459X; LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 NR 28 TC 147 Z9 147 U1 1 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2006 VL 131 IS 6 BP 2921 EP 2933 DI 10.1086/503704 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 051QT UT WOS:000238176400013 ER PT J AU Avrett, EH Kurucz, RL Loeser, R AF Avrett, E. H. Kurucz, R. L. Loeser, R. TI Identification of the broad solar emission features near 117 nm SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; atomic processes; line : identification; line : formation; radiative transfer; Sun : chromosphere ID CROSS-SECTION; ATOMIC SULFUR; CHROMOSPHERE; PHOTOIONIZATION; DYNAMICS AB Wilhelm et al. have recently called attention to the unidentified broad emission features near 117 nm in the solar spectrum. They discuss the observed properties of these features in detail but do not identify the source of this emission. We show that the broad autoionizing transitions of neutral sulfur are responsible for these emission features. Autoionizing lines of S I occur throughout the spectrum between Lyman alpha and the Lyman limit. Sulfur is a normal contributor to stellar spectra. We use non-LTE chromospheric model calculations with line data from the Kurucz 2004 S I line list to simulate the solar spectrum in the range 116 to 118 nm. We compare the results with SUMER disk-center observations from Curdt et al. and limb observations from Wilhelm et al. Our calculations generally agree with the SUMER observations of the broad autoionizing S I emission features, the narrow S I emission lines, and the continuum in this wavelength region, and agree with basic characteristics of the center-to-limb observations. In addition to modeling the average spectrum, we show that a change of +/- 200 K in the temperature distribution causes the intensity to change by a factor of 4. This exceeds the observed intensity variations 1) with time in quiet regions at these wavelengths, and 2) with position from cell centers to bright network. These results do not seem compatible with current dynamical models that have temporal variations of 1000 K or more in the low chromosphere. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Avrett, EH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM eavrett@cfa.harvard.edu; rkurucz@cfa.harvard.edu; rloeser@cfa.harvard.edu NR 17 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 JUN PY 2006 VL 452 IS 2 BP 651 EP 655 DI 10.1051/0004-6361:20065101 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 045NC UT WOS:000237747800034 ER PT J AU Crespo-Chacon, I Montes, D Garcia-Alvarez, D Fernandez-Figueroa, MJ Lopez-Santiago, J Foing, BH AF Crespo-Chacon, I Montes, D Garcia-Alvarez, D Fernandez-Figueroa, MJ Lopez-Santiago, J Foing, BH TI Analysis and modeling of high temporal resolution spectroscopic observations of flares on AD Leonis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : activity; stars : chromospheres; stars : flare; stars : late-type; stars : individual : AD Leo ID DIFFERENTIAL EMISSION MEASURE; EXTREME-ULTRAVIOLET EXPLORER; WHITE-LIGHT FLARES; LATE-TYPE STARS; X-RAY; ROTATIONAL MODULATION; STELLAR FLARES; XMM-NEWTON; DME STARS; UV CETI AB We report the results of a high temporal resolution spectroscopic monitoring of the flare star AD Leo. During 4 nights, more than 600 spectra were taken in the optical range using the Isaac Newton Telescope (INT) and the Intermediate Dispersion Spectrograph (IDS). We observed a large number of short and weak flares occurring very frequently (flare activity > 0.71 h(-1)). This is consistent with the very important role that flares can play in stellar coronal heating. The detected flares are non white-light flares and, although most solar flares are of this kind, very few such events have been observed previously in stars. The behaviour of different chromospheric lines (Balmer series from Ha to H-11, Ca II H & K, Na I D-1 and D-2, He I 4026 angstrom and He i D-3) was studied in detail for a total of 14 flares. We estimated the physical parameters of the flaring plasma by using a procedure that assumes a simplified slab model of flares. All the obtained physical parameters are consistent with previously derived values for stellar flares, and the areas - less than 2.3% of the stellar surface - are comparable with the size inferred for other solar and stellar flares. We studied the relationships between the physical parameters and the area, duration, maximum flux and energy released during the detected flares. C1 Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Armagh Observ, Armagh BT61 9DG, North Ireland. Osserv Astron Palermo, I-90134 Palermo, Italy. European Space Agcy, Estec, Div Res, Dept Space Sci,SCIR, NL-2200 AG Noordwijk, Netherlands. RP Crespo-Chacon, I (reprint author), Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain. EM icc@astrax.fis.ucm.es RI Montes, David/B-9329-2014; Fernandez-Figueroa, Maria Jose/C-3108-2017 OI Montes, David/0000-0002-7779-238X; Fernandez-Figueroa, Maria Jose/0000-0001-6892-198X NR 97 TC 17 Z9 17 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2006 VL 452 IS 3 BP 987 EP 1000 DI 10.1051/0004-6361:20053615 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 050VU UT WOS:000238117900031 ER PT J AU Hopkins, PF Narayan, R Hernquist, L AF Hopkins, Philip F. Narayan, Ramesh Hernquist, Lars TI How much mass do supermassive black holes eat in their old age? SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : active; galaxies : evolution; quasars : general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; ADVECTION-DOMINATED ACCRETION; QUASAR LUMINOSITY FUNCTION; X-RAY BINARIES; PARTICLE HYDRODYNAMICS SIMULATIONS; RADIATIVE-EFFICIENCY ACCRETION; SPECTRAL STATE TRANSITION; EMISSION-LINE LUMINOSITY; SAGITTARIUS-A-ASTERISK AB We consider the distribution of local supermassive black hole Eddington ratios and accretion rates, accounting for the dependence of radiative efficiency and bolometric corrections on the accretion rate. We find that black hole mass growth, both of the integrated mass density and the masses of most individual objects, must be dominated by an earlier, radiatively efficient, high accretion rate stage, and not by the radiatively inefficient low accretion rate phase in which most local supermassive black holes are currently observed. This conclusion is particularly true of supermassive black holes in elliptical host galaxies, as expected if they have undergone merger activity in the past that would fuel quasar activity and rapid growth. We discuss models of the time evolution of accretion rates and show that they all predict significant mass growth in a prior radiatively efficient state. The only way to avoid this conclusion is through careful fine-tuning of the accretion/quasar timescale to a value that is inconsistent with observations. Our results agree with a wide range of observational inferences drawn from the quasar luminosity function and X-ray background synthesis models, but our approach has the virtue of being independent of the modeling of source populations. Models in which black holes spend the great majority of their time in low accretion rate phases are thus completely consistent both with observations implying mass gain in relatively short, high accretion rate phases and with the local distribution of accretion rates. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 129 TC 69 Z9 69 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 JUN 1 PY 2006 VL 643 IS 2 BP 641 EP 651 DI 10.1086/503154 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700005 ER PT J AU Cox, TJ Di Matteo, T Hernquist, L Hopkins, PF Robertson, B Springel, V AF Cox, TJ Di Matteo, T Hernquist, L Hopkins, PF Robertson, B Springel, V TI X-ray emission from hot gas in galaxy mergers SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : evolution; galaxies : formation; galaxies : interactions; methods : n-body simulations; X-rays : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; QUASAR LUMINOSITY FUNCTION; XMM-NEWTON OBSERVATIONS; NGC-1316 FORNAX-A; CHANDRA OBSERVATIONS; ELLIPTIC GALAXIES; SHELL GALAXIES; BLACK-HOLES; STAR-FORMATION AB We examine X-ray emission produced from hot gas during collisions and mergers of disk galaxies. To study this process, we employ simulations that incorporate cosmologically motivated disk-galaxy models and include the effects of radiative cooling, star formation, supernova feedback, and accreting supermassive black holes. We find that during a merger, the colliding gas in the disks is shock heated to X-ray-emitting temperatures. The X-ray luminosity is spatially extended, rises during the initial stages of the merger, and peaks when the galactic centers coalesce. When a physical model for accreting black holes is included, the resulting feedback can drive powerful winds that contribute significantly to the amount and metallicity of hot gas, both of which increase the X-ray luminosity. In terms of their stellar kinematics and structural properties, the merger remnants in our simulations resemble elliptical galaxies. We find that the X-ray luminosities of the remnants with B-band luminosities in the range L-B similar to 10(10)-10(11) L-. are consistent with observations, while remnants with smaller or larger masses are underluminous in X-rays. Moreover, because the majority of the merger remnants are broadly consistent with the observed scaling relations between temperature, B-band luminosity, and X-ray luminosity, we conclude that major mergers are a viable mechanism for producing the X-ray halos of large, luminous elliptical galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Cox, TJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 78 TC 73 Z9 73 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2006 VL 643 IS 2 BP 692 EP 706 DI 10.1086/503284 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700011 ER PT J AU Chatzikos, M Sarazin, CL Kempner, JC AF Chatzikos, M Sarazin, CL Kempner, JC TI Chandra observation of Abell 2065: An unequal mass merger? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : clusters : individual (Abell 2065) radio continuum : galaxies; X-rays : galaxies : clusters ID GALAXY CLUSTERS; COOLING FLOWS; TEMPERATURE; PROFILES; CATALOG; A3667; CORES; ASCA AB We present an analysis of a 41 ks Chandra ACIS-I observation of the merging cluster Abell 2065. Previous ROSAT and ASCA observations provided evidence for an ongoing merger and suggested that there were two surviving cooling cores, which were associated with the two cD galaxies at the center of the cluster. The Chandra observation reveals only one X-ray surface brightness peak. Its gas is cool and displaced slightly from the more luminous, southern cD galaxy. Combined with the surface brightness profile, this suggests that this cool material has formed a cold front. In the higher spatial resolution Chandra image, the second feature to the north is not associated with the second cD; rather, it appears to be a trial of gas behind the main cD. We argue that only one of the two cooling cores has survived the merger. The survival of the cool core constrains the merger kinematics, placing an upper limit of less than or similar to 1900 km s(-1) on the relative merger velocity. A surface brightness discontinuity, found at similar to 140 kpc from the southern cD, has a Mach number of 1.66(-0.32)(+0.24) the nature of the discontinuity ( shock or cold front) is not clear fron the data. We argue that Abell 2065 is an unequal mass merger. The more massive southern cluster has driven a shock into the ICM of the infalling northern cluster, which has disrupted the cool core of the latter. We estimate that core crossing occurred a few hundred Myr ago, probably for the first time. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Bowdoin Coll, Dept Phys & Astron, Brunswick, ME 04011 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chatzikos, M (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM mnc3z@virginia.edu; sarazin@virginia.edu; jkempner@bowdoin.edu NR 19 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2006 VL 643 IS 2 BP 751 EP 763 DI 10.1086/503276 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700015 ER PT J AU Finoguenov, A Henriksen, MJ Miniati, F Briel, UG Jones, C AF Finoguenov, A Henriksen, MJ Miniati, F Briel, UG Jones, C TI A puzzling merger in A3266: The hydrodynamic picture from XMM-Newton SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (Abell 3266); intergalactic medium; X-rays : galaxies : clusters ID CLUSTER SCALING PROJECT; DXL GALAXY CLUSTERS; INTRACLUSTER MEDIUM; EVOLUTION; TEMPERATURE; ENTROPY; DYNAMICS; CORES; MAPS AB Using a mosaic of nine XMM-Newton observations, we study the hydrodynamic state of the merging cluster of galaxies Abell 3266. The high signal-to-noise ratio of spectroscopic data of XMM-Newton allows us to determine the thermodynamic conditions of the intracluster medium on similar to 50 kpc scales. High statistical quality X-ray data reveal the presence of an extended region of low-entropy gas ( LEG) running northeast from the primary cluster core along the nominal merger axis. The LEG is a major feature distinguishing the merger event in A3266 from other clusters. The mass of the low-entropy gas is similar to 1.3 x10(13) M-.. We test the possibility that the origin of the observed low-entropy gas is related either to the disruption of a preexisting cooling core in Abell 3266 or to the stripping of gas from an infalling subcluster. We find that the low-entropy gas has a metallicity 1.5 - 2 times higher than the bulk of the cluster, yet lower than one-half the solar value typical for the cool cores. In addition, both the radial pressure and entropy profiles, as well as the iron abundance of Abell 3266, do not resemble those in other known cool core clusters ( e. g., Abell 478). Thus, we conclude that our observations favor a scenario in which the low-entropy region corresponds to subcluster gas stripped from its dark matter halo. In this scenario the subcluster would be falling onto the core of A3266 from the foreground, having a velocity component in the observer plane toward the southwest. The arguments based on both velocity dispersion and gas mass measurements suggest a mass ratio in the merger of 1:10. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Finoguenov, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. NR 32 TC 18 Z9 18 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2006 VL 643 IS 2 BP 790 EP 796 DI 10.1086/503285 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700017 ER PT J AU Ridge, NA Schnee, SL Goodman, AA Foster, JB AF Ridge, NA Schnee, SL Goodman, AA Foster, JB TI The complete nature of the warm dust shell in Perseus SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; HII regions; infrared : ISM; ISM : individual (G159.6-18.5); radio lines : ISM ID STAR-FORMING REGIONS; MIDCOURSE-SPACE-EXPERIMENT; DARK CLOUD COMPLEX; INTERSTELLAR EXTINCTION; EMISSION; TAURUS; MAPS; OPHIUCHUS; NGC-1333; NEBULAE AB The Perseus molecular cloud complex is a greater than or similar to 30 pc long chain of molecular clouds most well known for the two star-forming clusters NGC 1333 and IC 348 and the well-studied outflow source in B5. However, when studied at mid- to far-infrared wavelengths, the region is dominated by a similar to 10 pc diameter shell of warm dust, likely generated by an H II region caused by the early-B star HD 278942. Using a revised calibration technique the COMPLETE team has produced high-sensitivity temperature and column density maps of the Perseus region from IRAS Sky Survey Atlas (ISSA) 60 and 100 mu m data. In this paper, we combine the ISSA-based dust-emission maps with other observations collected as part of the COMPLETE Survey, along with archival H alpha and MSX observations. Molecular line observations from FCRAO and extinction maps constructed by applying the NICER method to the 2MASS catalog provide independent estimates of the "true" column density of the shell. H alpha emission in the region of the shell confirms that it is most likely an H II region located behind the cloud complex, and 8 mu m data from MSX indicate that the shell may be interacting with the cloud. Finally, the two polarization components seen toward background stars in the region by Goodman et al. can be explained by the association of the stronger component with the shell. If confirmed, this would be the first observation of a parsec-scale swept-up magnetic field. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ridge, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nridge@cfa.harvard.edu; sschnee@cfa.harvard.edu; agoodman@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 38 TC 36 Z9 36 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2006 VL 643 IS 2 BP 932 EP 944 DI 10.1086/502957 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700027 ER PT J AU Rho, J Reach, WT Lefloch, B Fazio, GG AF Rho, Jeonghee Reach, William T. Lefloch, Bertrand Fazio, Giovanni G. TI Spectacular Spitzer images of the Trifid Nebula: Protostars in a young, massive-star-forming region SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; infrared : stars; ISM : individual (Trifid Nebula); stars : formation ID INFRARED ARRAY CAMERA; SPACE-TELESCOPE; PROTOSTELLAR OBJECTS; CONTINUUM EMISSION; INTERSTELLAR DUST; CORES; EXTINCTION; TURBULENT AB Spitzer IRAC and MIPS images of the Trifid Nebula (M20) reveal its spectacular appearance in infrared light, highlighting the nebula's special evolutionary stage. The images feature recently formed massive protostars and numerous young stellar objects, and a single O star that illuminates the surrounding molecular cloud from which it formed, and unveil large-scale, filamentary dark clouds. Multiple protostars are detected in the infrared, within the cold dust cores of TC3 and TC4, which were previously defined as Class 0. The cold dust continuum cores of TC1 and TC2 contain only one protostar each. The Spitzer color-color diagram allowed us to identify similar to 160 young stellar objects (YSOs) and classify them into different evolutionary stages. The diagram also revealed a unique group of YSOs that are bright at 24 mu m but have the spectral energy distribution peaking at 5-8 mu m. Despite expectation that Class 0 sources would be "starless" cores, the Spitzer images, with unprecedented sensitivity, uncover mid-infrared emission from these Class 0 protostars. The mid-infrared detections of Class 0 protostars show that the emission escapes the dense, cold envelope of young protostars. The mid-infrared emission of the protostars can be fit by two temperatures of 150 and 400 K; the hot core region is probably optically thin in the mid-infrared regime, and the size of hot core is much smaller than that of the cold envelope. The presence of multiple protostars within the cold cores of Class 0 objects implies that clustering occurs at this early stage of star formation. The most massive star in the TC3 cluster is located at the center of the cluster and at the bottom of the gravitational potential well. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rho, J (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM rho@ipac.caltech.edu; reach@ipac.caltech.edu; lefloch@obs.ujf-grenoble.fr; gfazio@cfa.harvard.edu OI Reach, William/0000-0001-8362-4094 NR 31 TC 32 Z9 32 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 JUN 1 PY 2006 VL 643 IS 2 BP 965 EP 977 DI 10.1086/503245 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700030 ER PT J AU Muzerolle, J Adame, L D'Alessio, P Calvet, N Luhman, KL Muench, AA Lada, CJ Rieke, GH Siegler, N Trilling, DE Young, ET Allen, L Hartmann, L Megeath, ST AF Muzerolle, James Adame, Lucia D'Alessio, Paola Calvet, Nuria Luhman, Kevin L. Muench, August A. Lada, Charles J. Rieke, George H. Siegler, Nick Trilling, David E. Young, Erick T. Allen, Lori Hartmann, Lee Megeath, S. Thomas TI 24 mu m detections of circum(sub) stellar disks in IC 348: Grain growth and inner holes? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; infrared : stars; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID LOW-MASS STARS; YOUNG BROWN DWARFS; T-TAURI STARS; MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; ACCRETION DISKS; PROTOPLANETARY DISKS; SUBSTELLAR OBJECTS; IRS SPECTRA; GM-AURIGAE AB We present observations of six late-type members of the young cluster IC 348 detected at 24 mu m with the Multiband Imaging Photometer for Spitzer (MIPS). At least four of the objects are probably substellar. Combining these data with ground-based optical and near-infrared photometry and complementary observations with the Infrared Array Camera (IRAC), we have modeled the spectral energy distributions using detailed models of irradiated accretion disks. We are able to fit the observations with models using a range of maximum grain sizes from ISM-type dust to grains as large as 1 mm. Two objects show a lack of excess emission at wavelengths shortward of 5.8-8 mu m but significant excess at longer wavelengths, indicative of large optically thin or evacuated inner holes. Our models indicate an inner hole of radius similar to 0.5-0.9 AU for the brown dwarf L316; this is the first brown dwarf with evidence for an AU-scale inner disk hole. We examine several possible mechanisms for the inner disk clearing in this case, including photoevaporation and planet formation. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Univ Michigan, Ann Arbor, MI 48109 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 56 TC 45 Z9 45 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2006 VL 643 IS 2 BP 1003 EP 1010 DI 10.1086/503271 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053XF UT WOS:000238338700034 ER PT J AU Karastergiou, A Neri, R Gurwell, MA AF Karastergiou, A Neri, R Gurwell, MA TI Adapting and expanding interferometric arrays SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation : interferometers; methods : numerical ID DESIGN AB We outline here a simple yet efficient method for finding optimized configurations of the elements of radio-astronomical interferometers with fixed pad locations. The method can be successfully applied, as we demonstrate, to define new configurations when changes to the array take place. This may include the addition of new pads or new antennas, or the loss of pads or antennas. Our method is based on identifying which placement of elements provides the most appropriate u-v plane sampling for astronomical imaging. C1 IRAM, St Martin Dheres, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karastergiou, A (reprint author), IRAM, 300 Rue Piscine,Domaine Univ, St Martin Dheres, France. NR 13 TC 3 Z9 3 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2006 VL 164 IS 2 BP 552 EP 558 DI 10.1086/503630 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 053NT UT WOS:000238312500009 ER PT J AU Reeves, RG Bermingham, E AF Reeves, RG Bermingham, E TI Colonization, population expansion, and lineage turnover: phylogeography of Mesoamerican characiform fish SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE ATPase; mitochondrial DNA; niche-overlap; phylogeography; polytomies; primary freshwater fish; priority effect; synonymous substitution ID FRESH-WATER FISHES; MITOCHONDRIAL-DNA; CENTRAL-AMERICA; LIMITING SIMILARITY; ICE AGES; DIVERGENCE; SPECIATION; PANAMA; NUCLEOTIDE; EVOLUTION AB We present a phylogeographical analysis of four genera of Mesoamerican primary freshwater fish (Brycon, Bryconamericus, Eretmobrycon, and Cyphocharax). Three hundred and thirty-nine individuals were genotyped into one of 31 operational taxonomic units (OTUs) based on the nucleotide sequence of their mitochondrial ATPase 6 & 8 genes (842-839 bp). Contrary to inference based on the species-level taxonomy of these genera, molecular data identified only a single case of sympatry between closely related OTUs, despite extensive parapatry. Polytomies dominate the mtDNA-based phylogenies and demonstrate multiple, noncontemporaneous waves of rapid expansion across Mesoamerica from South American sources. Analyses based on genetic distances observed among congeneric species of Mesoamerican primary freshwater fishes in comparison to divergence between transisthmian marine fishes permit the strong inference that the Pliocene rise of the Panama land bridge provided the first opportunity for the colonization of Mesoamerica by Characiform fishes. We develop a priority-effect model, based on the assumption that genetically closely related OTUs share similar ecological niches, to reconcile the general lack of contemporary sympatry between closely related OTUs with the substantial historical connectivity among Mesoamerican drainages demonstrated by the rapid expansion of Brycon, Bryconamericus, and Cyphocharax. Finally, in most cases, we infer that the westerly limits of freshwater fish distributions in Mesoamerica are more consistent with being defined by ecological factors rather than by dispersal limitation. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Newcastle Upon Tyne, Dept Nutrit & Biol Sci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. RP Bermingham, E (reprint author), Smithsonian Trop Res Inst, Apto 2072, Balboa, Panama. EM eb@naos.si.edu NR 64 TC 32 Z9 34 U1 0 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JUN PY 2006 VL 88 IS 2 BP 235 EP 255 DI 10.1111/j.1095-8312.2006.00619.x PG 21 WC Evolutionary Biology SC Evolutionary Biology GA 047HZ UT WOS:000237871700008 ER PT J AU Bi, YM Nielsen, KL Kilts, TM Yoon, A Karsdal, MA Wimer, HF Greenfield, EM Heegaard, AM Young, MF AF Bi, YM Nielsen, KL Kilts, TM Yoon, A Karsdal, MA Wimer, HF Greenfield, EM Heegaard, AM Young, MF TI Biglycan deficiency increases osteoclast differentiation and activity due to defective osteoblasts SO BONE LA English DT Article DE biglycan; proteoglycan; osteoclast; osteolysis; ECM ID LEUKOCYTE PROTEASE INHIBITOR; BONE-RESORPTION; MICE LACKING; IN-VITRO; EXPRESSION; CELLS; GENE; OSTEOPOROSIS; OSTEOPONTIN; RAT AB Bone mass is maintained by a fine balance between bone formation by osteoblasts and bone resorption by osteoclasts. Although osteoblasts and osteoclasts have different developmental origins, it is generally believed that the differentiation, function, and survival of osteoclasts are regulated by osteogenic cells. We have previously shown that the extracellular matrix protein, biglycan (Bgn), plays an important role in the differentiation of osteoblast precursors. In this paper, we showed that Bgn is involved in regulating osteoclast differentiation through its effect on osteoblasts and their precursors using both in vivo and in vitro experiments. The in vivo osteolysis experiment showed that LPS (lipopolisaccharide)-induced osteolysis occurred more rapidly and extensively in bgn deficient mice compared to wild type (WT) mice. To further understand the mechanism of action, we determined the effects of Bgn on la, 25-dihydroxyvitamin D-3 (1,25-(OH)(2)D-3)-induced osteoclast differentiation and bone resorption in an co-culture of calvariae-derived pre-osteoblasts and osteoclast precursors derived from spleen or bone marrow. Time course and dose response experiments showed that tartrate-resistant acid phosphatase-positive multinuclear cells appeared earlier and more extensively in the co-cultures containing calvarial cells from bgn deficient mice than WT mice, regardless of the genotype of osteoclast precursors. The osteoblast abnormality that stimulated osteoclast formation appeared to be independent of the differential production of soluble RANKL and OPG and, instead, due to a decrease in osteoblast maturation accompanied by increase in osteoblastic proliferation. In addition to the imbalance between differentiation and proliferation, there was a differential decrease in secretory leukocyte protease inhibitor (slpi) in bgn deficient osteoblasts treated with 1,25-(OH)(2)D-3. These findings point to a novel molecular factor made by osteoblasts that could potentially be involved in LPS-induced osteolysis. Published by Elsevier Inc. C1 Natl Inst Dent & Craniofacial Res, NIH, Craniofacial & Skeletal Dis Branch, Bethesda, MD 20892 USA. Natl Univ Hosp, Finsen Ctr, Nordic Biosci AS, Copenhagen, Denmark. Natl Univ Hosp, Finsen Ctr, Dept Radiat Biol, Copenhagen, Denmark. Case Western Reserve Univ, Dept Orthopaed, Cleveland, OH 44106 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Young, MF (reprint author), Natl Inst Dent & Craniofacial Res, NIH, Craniofacial & Skeletal Dis Branch, Bldg 30 Room 225,MSC 4320,9000 Rockville Pike, Bethesda, MD 20892 USA. EM myoung@dir.nidcr.nih.gov FU Intramural NIH HHS NR 41 TC 45 Z9 47 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 J9 BONE JI Bone PD JUN PY 2006 VL 38 IS 6 BP 778 EP 786 DI 10.1016/j.bone.2005.11.005 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 055DB UT WOS:000238429100004 PM 16364709 ER PT J AU Chamorro-Lacayo, ML Konstantinov, AS Moseyko, AG AF Chamorro-Lacayo, M. Lourdes Konstantinov, Alexander S. Moseyko, Alexey G. TI Comparative morphology of the female genitalia and some abdominal structures of Neotropical Cryptocephalini (Coleoptera : Chrysomelidae : Cryptocephalinae) SO COLEOPTERISTS BULLETIN LA English DT Article ID FLEA BEETLES COLEOPTERA AB The female genitalia of New World Cryptocephalini was studied and illustrated based on representatives of 11 of the 13 genera of the tribe. It was found that female genitalia contain pleutites IX, a rare and apparently primitive feature among leaf beetles. In other features cryptocephaline female genitalia are simpler than genitalia of other leaf beetles in having a poorly sclerotized sternite VIII and lacking the tignum. It is also hypothesized that the vagina is formed by sternites IX (dorsally) and VIII (ventrally), and that sclerotized plate of sternite IX can be homologized with vaginal palpi of flea beetles. A set of characters of diagnostic and of possible phylogenetic value was found. In general, Cryptocephalina and Monachulina bear the greatest affinity in overall morphology of the female genitalia, with Pachybrachina possessing a different set of unique morphological states. Of particular diagnostic and phylogenetic value at the subtribal level, as revealed by this study, are the shape and degree of sclerotization of tergite VIII, tergite IX, and sternite VIII. C1 Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. USDA, Systemat Entomol Lab, Natl Museum Nat Hist, Agr Res Serv,Smithsonian Inst,PSI, Washington, DC 20013 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Chamorro-Lacayo, ML (reprint author), Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. EM cham0138@umn.edu; akonstan@sel.barc.usda.gov; moseyko@mail333.com RI Moseyko, Alexey/R-5297-2016 NR 27 TC 12 Z9 12 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X EI 1938-4394 J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 2006 VL 60 IS 2 BP 113 EP 134 DI 10.1649/873.1 PG 22 WC Entomology SC Entomology GA 098UV UT WOS:000241549200005 ER PT J AU Nascimento, HEM Andrade, ACS Camargo, JLC Laurnce, WF Laurance, SG Ribeiro, JEL AF Nascimento, Henrique E. M. Andrade, Ana C. S. Camargo, Jose Luis C. Laurnce, William F. Laurance, Susan G. Ribeiro, Jose Eduardo L. TI Effects of the surrounding matrix on tree recruitment in Amazonian forest fragments SO CONSERVATION BIOLOGY LA English DT Article DE Amazon; edge effects; forest fragmentation; pioneer species; rain forest ID TROPICAL RAIN-FOREST; PIONEER TREES; SPECIES RICHNESS; SEED DISPERSAL; COMMUNITIES; VEGETATION; REGENERATION; DYNAMICS; PATTERNS; GROWTH AB Little is known about how the surrounding modified matrix affects tree recruitment infragmented forests. We contrasted effects of two different matrix types, Vismia- and Cecropia-dominated regrowth, on recruitment of pioneer tree species in forest fragments in central Amazonia. Our analyses were based on 22, 1-ha plots in seven experimental forest fragments ranging in size from I to 100 ha. By 13 to 17 years after fragmentation, the population density of pioneer trees was significantly higher in plots surrounded by Vismia regrowth than in plots surrounded by Cecropia regrowth, and the species composition and dominance of pioneers differed markedly between the two matrix types. Cecropia sciadophylla was the most abundant pioneer in fragments surrounded by Cecropia regrowth (constituting nearly 50% of all pioneer trees), whereas densities of species in Vismia-surrounded fragments were distributed more evenly. Thus the surrounding matrix had a strong influence on patterns of tree recruitment in Amazonian forest fragments. C1 Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. INPA, Dept Bot, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. RP Nascimento, HEM (reprint author), Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM henrique@inpa.gov.br RI Nascimento, Henrique/F-8612-2012; Laurance, Susan/G-6021-2011; Camargo, Jose Luis/C-3137-2015; Lahoz da Silva Ribeiro, Jose Eduardo/A-8574-2013 OI Laurance, Susan/0000-0002-2831-2933; Lahoz da Silva Ribeiro, Jose Eduardo/0000-0002-2389-5631 NR 61 TC 37 Z9 38 U1 7 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2006 VL 20 IS 3 BP 853 EP 860 DI 10.1111/j.1523-1739.2006-00344.x PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 053NZ UT WOS:000238313200044 PM 16909577 ER PT J AU Hagedorn, M Carter, VL Steyn, RA Krupp, D Leong, JC Lang, RP Tiersch, TR AF Hagedorn, M Carter, VL Steyn, RA Krupp, D Leong, JC Lang, RP Tiersch, TR TI Preliminary studies of sperm cryopreservation in the mushroom coral, Fungia scutaria SO CRYOBIOLOGY LA English DT Article DE coral; sperm; cryoprotectants; genetic banking ID CRASSOSTREA-GIGAS; PACIFIC OYSTER; SPERMATOZOA AB Coral species throughout the world are facing severe environmental pressures. Because of this, we began cryobiological studies on the sperm of the mushroom coral, Fungia scutaria. We determined that F scutaria sperm had a mean length of 56 mu m and head diameter of 2.5 mu m, and a mean spontaneous ice nucleation temperature of -37.2 +/- 1.7 degrees C. When the sperm were exposed to the cryoprotectant glycerol for 5 or 20 min (at 10% v/v), no fertilized larvae were produced. However, when sperm were exposed for 20 min to propylene glycol (10% v/v), fertilizations were produced at the same rate as untreated control eggs and sperm (P > 0.05), but slightly less for dimethyl sulfoxide (10% v/v) (P < 0.05). Regardless, dimethyl sulfoxide caused less osmotic damage to the sperm membrane than did propylene glycol. Therefore, we used the dimethyl sulfoxide (10% v/v) to develop cryopreservation protocols that yielded good post-thaw morphology and motility (> 95%) for coral sperm. (c) 2006 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. Oregon State Univ, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. Louisiana State Univ, Ctr Agr, Louisiana Agr Expt Stn, Aquaculture Res Stn, Baton Rouge, LA 70803 USA. RP Hagedorn, M (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. EM hagedornm@si.edu NR 12 TC 22 Z9 22 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD JUN PY 2006 VL 52 IS 3 BP 454 EP 458 DI 10.1016/j.cryobiol.2006.03.001 PG 5 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 051OE UT WOS:000238169600014 PM 16626677 ER PT J AU Hubbell, SP AF Hubbell, Stephen P. TI Neutral theory and the evolution of ecological equivalence SO ECOLOGY LA English DT Article DE Barro Colorado Island; ecological equivalence; neutral theory; niche differentiation; shade tolerance; tropical tree communities ID RECRUITMENT LIMITATION; NEOTROPICAL FOREST; COMMUNITY ECOLOGY; SPECIES ABUNDANCE; TROPICAL FORESTS; SAPLING GROWTH; DIVERSITY; BIODIVERSITY; HYPOTHESIS; COMPETITION AB Since the publication of the unified neutral theory in 2001, there has been much discussion of the theory, pro and con. The hypothesis of ecological equivalence is the fundamental yet controversial idea behind neutral theory. Assuming trophically similar species are demographically alike (symmetric) on a per capita basis is only an approximation, but it is equivalent to asking: How many of the patterns of ecological communities are the result of species similarities, rather than of species differences? The strategy behind neutral theory is to see how far one can get with the simplification of assuming ecological equivalence before introducing more complexity. In another paper, I review the empirical evidence that led me to hypothesize ecological equivalence among many of the tree species in the species-rich tropical forest on Barro Colorado Island (BCI). In this paper, I develop a simple model for the evolution of ecological equivalence or niche convergence, using as an example evolution of the suite of life history traits characteristic of shade tolerant tropical tree species. Although the model is simple, the conclusions from it seem likely to be robust. I conclude that ecological equivalence for resource use are likely to evolve easily and often, especially in species-rich communities that are dispersal and recruitment limited. In the case of the BCI forest, tree species are strongly dispersal- and recruitment-limited, not only because of restricted seed dispersal, but also because of low recruitment success due to heavy losses of the seedling stages to predators and pathogens and other abiotic stresses such as drought. These factors and the high species richness of the community strongly reduce the potential for competitive exclusion of functionally equivalent or nearly equivalent species. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30605 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Hubbell, SP (reprint author), Univ Georgia, Dept Plant Biol, Athens, GA 30605 USA. EM shubbell@plantbio.uga.edu NR 58 TC 212 Z9 249 U1 17 U2 179 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2006 VL 87 IS 6 BP 1387 EP 1398 DI 10.1890/0012-9658(2006)87[1387:NTATEO]2.0.CO;2 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 058IJ UT WOS:000238658400006 PM 16869413 ER PT J AU Hines, J Megonigal, JP Denno, RF AF Hines, J Megonigal, JP Denno, RF TI Nutrient subsidies to belowground microbes impact aboveground food web interactions SO ECOLOGY LA English DT Article DE aboveground-belowground interactions; detritus; food web dynamics; insect herbivores; intertidal cord grass; nitrogen mineralization; nutrient subsidies; plant-insect interactions; predation; soil microbes; Spartina alterniflora ID BOTTOM-UP FORCES; SALT-MARSH; SPARTINA-ALTERNIFLORA; TOP-DOWN; TERRESTRIAL ECOSYSTEMS; RELATIVE STRENGTH; INSECT HERBIVORES; SMOOTH CORDGRASS; NATURAL ENEMIES; PLANT NITROGEN AB Historically, terrestrial food web theory has been compartmentalized into interactions among aboveground or belowground communities. In this study we took a more synthetic approach to understanding food web interactions by simultaneously examining four trophic levels and investigating how nutrient ( nitrogen and carbon) and detrital subsidies impact the ability of the belowground microbial community to alter the abundance of aboveground arthropods ( herbivores and predators) associated with the intertidal cord grass Spartina alterniflora. We manipulated carbon, nitrogen, and detrital resources in a field experiment and measured decomposition rate, soil nitrogen pools, plant biomass and quality, herbivore density, and arthropod predator abundance. Because carbon subsidies impact plant growth only indirectly ( microbial pathways), whereas nitrogen additions both directly ( plant uptake) and indirectly ( microbial pathways) impact plant primary productivity, we were able to assess the effect of both belowground soil microbes and nutrient availability on aboveground herbivores and their predators. Herbivore density in the field was suppressed by carbon supplements. Carbon addition altered soil microbial dynamics ( net potential ammonification, litter decomposition rate, DON [dissolved organic N] concentration), which limited inorganic soil nitrogen availability and reduced plant size as well as predator abundance. Nitrogen addition enhanced herbivore density by increasing plant size and quality directly by increasing inorganic soil nitrogen pools, and indirectly by enhancing microbial nitrification. Detritus adversely affected aboveground herbivores mainly by promoting predator aggregation. To date, the effects of carbon and nitrogen subsidies on salt marshes have been examined as isolated effects on either the aboveground or the belowground community. Our results emphasize the importance of directly addressing the soil microbial community as a factor that in. uences aboveground food web structure by affecting plant size and aboveground plant nitrogen. C1 Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. Smithsonian Environm Res Ctr, Edgewater, MD 20912 USA. RP Hines, J (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. EM hines@umd.edu NR 77 TC 27 Z9 29 U1 5 U2 53 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD JUN PY 2006 VL 87 IS 6 BP 1542 EP 1555 DI 10.1890/0012-9658(2006)87[1542:NSTBMI]2.0.CO;2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 058IJ UT WOS:000238658400023 PM 16869430 ER PT J AU Mitchell, CE Agrawal, AA Bever, JD Gilbert, GS Hufbauer, RA Klironomos, JN Maron, JL Morris, WF Parker, IM Power, AG Seabloom, EW Torchin, ME Vazquez, DP AF Mitchell, CE Agrawal, AA Bever, JD Gilbert, GS Hufbauer, RA Klironomos, JN Maron, JL Morris, WF Parker, IM Power, AG Seabloom, EW Torchin, ME Vazquez, DP TI Biotic interactions and plant invasions SO ECOLOGY LETTERS LA English DT Review ID INCREASED COMPETITIVE ABILITY; ARBUSCULAR MYCORRHIZAL FUNGI; ENEMY RELEASE HYPOTHESIS; BIOLOGICAL-CONTROL; AMMOPHILA-ARENARIA; INTRODUCED POPULATIONS; EVOLUTIONARY ECOLOGY; HERBIVOROUS INSECTS; SPECIES COEXISTENCE; CENTAUREA-MACULOSA AB Introduced plant populations lose interactions with enemies, mutualists and competitors from their native ranges, and gain interactions with new species, under new abiotic conditions. From a biogeographical perspective, differences in the assemblage of interacting species, as well as in abiotic conditions, may explain the demographic success of the introduced plant populations relative to conspecifics in their native range. Within invaded communities, the new interactions and conditions experienced by the invader may influence both its demographic success and its effects on native biodiversity. Here, we examine indirect effects involving enemies, mutualists and competitors of introduced plants, and effects of abiotic conditions on biotic interactions. We then synthesize ideas building on Darwin's idea that the kinds of new interactions gained by an introduced population will depend on its relatedness to native populations. This yields a heuristic framework to explain how biotic interactions and abiotic conditions influence invader success. We conclude that species introductions generally alter plants' interactions with enemies, mutualists and competitors, and that there is increasing evidence that these altered interactions jointly influence the success of introduced populations. C1 Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. Univ N Carolina, Curriculum Ecol, Chapel Hill, NC 27599 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. Colorado State Univ, Dept Bioagr Sci & Pest Management, Ft Collins, CO 80523 USA. Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. Duke Univ, Dept Biol, Durham, NC 27708 USA. Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Ctr Reg Invest Cient & Tecnol, Inst Argentino Invest Zonas Aridas, RA-5500 Mendoza, Argentina. RP Mitchell, CE (reprint author), Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. EM mitchell@bio.unc.edu RI Mitchell, Charles/I-3709-2014; OI Mitchell, Charles/0000-0002-1633-1993; Seabloom, Eric/0000-0001-6780-9259; Vazquez, Diego P./0000-0002-3449-5748 NR 116 TC 348 Z9 359 U1 23 U2 259 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD JUN PY 2006 VL 9 IS 6 BP 726 EP 740 DI 10.1111/j.1461-0248.2006.00908.x PG 15 WC Ecology SC Environmental Sciences & Ecology GA 043YD UT WOS:000237638000008 PM 16706916 ER PT J AU Pardo-de-Santayana, M Tardio, J Heinrich, M Touwaide, A Morales, R AF Pardo-de-Santayana, Manuel Tardio, Javier Heinrich, Michael Touwaide, Alain Morales, Ramon TI Plants in the works of Cervantes SO ECONOMIC BOTANY LA English DT Article DE cervantes; literary texts; ethnobotany; history of plant uses; Spain ID SPAIN AB We searched this and the other works of Cervantes for references to plants, plant communities, and products. These texts capture the customs, thoughts, beliefs, and traditions of Spanish culture in the late 16th and early 17th centuries. They also repeat literary themes of ancient Greek and Roman literature. Plant citations were grouped in three categories: plants as part of the environment, useful plants, and plants in symbolic expressions. A total of 150 species were registered, 102 of which appear in Don Quijote. The taxa with the highest frequency of occurrence are Vitis vinifera, Phoenix dactylifera, Triticum aestivum, Laurus nobilis, Rosa spp., Olea europaea, Quercus ilex, and Arundo donax. The number of references to plants and the variety of species seem to attest to a sound and intimate knowledge of plants, their relevance as a landscape feature, and their utility. Many edible, ornamental, technological, and medicinal plants are referred to either explicitly or implicitly. Several species are mentioned in a figurative sense through references to their symbolic meaning, in proverbs, idiomatic expressions, metaphors, or by mentioning them in comparisons and literary figures of speech. C1 Univ London, Sch Pharm, Ctr Pharmacognosy & Phytotherapy, London WC1N 1AX, England. CSIS, Real Jardin Bot, E-28014 Madrid, Spain. INIDRA, E-28800 Madrid, Spain. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Pardo-de-Santayana, M (reprint author), Univ London, Sch Pharm, Ctr Pharmacognosy & Phytotherapy, 29-39 Brunswick Sq, London WC1N 1AX, England. EM mpardo@marjb.csic.es RI Pardo-de-Santayana, Manuel/A-1123-2012; Heinrich, Michael/C-3727-2013; Tardio, Javier/L-2880-2014; Morales, Ramon/K-2262-2014 OI Pardo-de-Santayana, Manuel/0000-0001-9406-4758; Heinrich, Michael/0000-0003-2611-6303; Tardio, Javier/0000-0003-1690-1666; Morales, Ramon/0000-0003-2343-9158 NR 48 TC 10 Z9 13 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0013-0001 J9 ECON BOT JI Econ. Bot. PD SUM PY 2006 VL 60 IS 2 BP 159 EP 181 DI 10.1663/0013-0001(2006)60[159:PITWOC]2.0.CO;2 PG 23 WC Plant Sciences SC Plant Sciences GA 063PP UT WOS:000239032300005 ER PT J AU Leshin, LA Vicenzi, E AF Leshin, Laurie A. Vicenzi, Edward TI Aqueous processes recorded by Martian meteorites: Analyzing Martian water on Earth SO ELEMENTS LA English DT Article DE Mars; meteorites; stable isotopes; carbonates; water-rock interaction ID SNC METEORITES; ISOTOPIC COMPOSITION; MARS; ALH84001; LAFAYETTE; HYDROGEN; CARBONATE; NAKHLA; ATMOSPHERE; EVOLUTION AB Martian meteorites have delivered to Earth water molecules and minerals produced by aqueous processes on Mars. The study of these samples, using powerful analytical instrumentation, provides a basis for understanding aqueous activity on Mars. Although most analyses are at the scale of microns, the conclusions reached have important implications for large-scale aqueous processes. Secondary minerals, such as clays, salts, and carbonates, are present at some level in all Martian meteorite subtypes and are especially important in the nakhlites and ALH84001. Light element stable isotope analyses show evidence for mixing between atmosphere and magmatic fluids into a crustal reservoir, and that this crustal water was not in equilibrium with the host rocks. The mineralogical and isotopic data present a fairly consistent picture of the aqueous history of Mars: low levels of aqueous alteration are generally present but extensive aqueous processes are probably limited in space and time. C1 NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Mineral Sci, Washington, DC 20560 USA. RP Leshin, LA (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. EM laurie.leshin@nasa.gov; vicenzi@volcano.si.edu NR 34 TC 21 Z9 21 U1 1 U2 13 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 EI 1811-5217 J9 ELEMENTS JI Elements PD JUN PY 2006 VL 2 IS 3 BP 157 EP 162 DI 10.2113/gselements.2.3.157 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 052OW UT WOS:000238244000009 ER PT J AU Russell, MJ Montagna, PA Kalke, RD AF Russell, MJ Montagna, PA Kalke, RD TI The effect of freshwater inflow on net ecosystem metabolism in Lavaca Bay, Texas SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE net ecosystem metabolism; estuarine metabolic rates; freshwater inflow; impairment; indicators; ecological indicators ID ORGANIC-MATTER; CHESAPEAKE BAY; DISSOLVED-OXYGEN; US ESTUARIES; RESPIRATION; EUTROPHICATION; DEPLETION; SEDIMENT; DYNAMICS; EXCHANGE AB Estuaries and other coastal ecosystems depend on freshwater inflow to maintain the gradients in environmental characteristics that define these transitional water bodies. Freshwater inflow (FWI) rates in many estuaries are changing due to changing land use patterns, water diversions for human consumption, and climate effects, but there are no standard criteria to determine minimum inflow rates. An ecological indicator is required so models can be produced to predict how changing hydrology might affect estuarine metabolic rates, productivity, or impairment. One indicator of estuarine metabolic rates is net ecosystem metabolism (NEM). It is hypothesized that metabolic rates (as indicated by NEM) will depend on recently delivered FWI. To test this hypothesis, daily NEM was calculated from high frequency changes in dissolved oxygen measurements in a shallow water estuary, Lavaca Bay, Texas, USA and related to FWI and other environmental conditions. There was a significant relationship between NEM and cumulative ten-day FWI in upper Lavaca Bay, with more heterotrophic conditions occurring after high FWI events. No significant relationship existed between NEM and FWI in lower Lavaca Bay, where other environmental conditions, such as tidal forcing, may be more influential. An empirical model simulating NEM's response to FWI in upper Lavaca Bay was more accurate during moderate to high flows than during low base-flow conditions. Thus, quantity of FWI and distance from the inflow point source constrained the dependence of NEM on FWI. NEM can be quite variable over time and within a bay dominated by a river at one end and ocean exchange at the other end. The range of environmental gradients over time and within an estuary will determine how representative NEM at a single location is for an entire estuary. However, during high flow period pulses NEM can accurately predict shifts from balanced to heterotrophic conditions. Therefore, use of the NEM model as an indicator of FWI effects is constrained to regions in estuaries that are most effected by FWI because of proximity to the source or the size of FWI pulse events. The unique geologic, geographic, and climate signature's of individual estuaries will dictate the fit of this model in space and time. Inclusion of other environmental factors, such as temperature or irradiance, is necessary to improve the NEM model during low base-flow conditions. It is concluded that the NEM model does provide a useful indicator of FWI effects on ecosystem metabolic rates as it works well in the upper regions of Lavaca Bay and during freshwater inflow pulses where and when freshwater inflow has more influence than other environmental factors. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Texas, Inst Marine Sci, Port Aransas, TX 78373 USA. RP Russell, MJ (reprint author), Smithsonian Environm Res Inst, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21027 USA. EM russellm@si.edu RI Ross, Donald/F-7607-2012 OI Ross, Donald/0000-0002-8659-3833 NR 48 TC 33 Z9 34 U1 1 U2 19 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD JUN PY 2006 VL 68 IS 1-2 BP 231 EP 244 DI 10.1016/j.ecss.2006.02.005 PG 14 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 057OG UT WOS:000238604500021 ER PT J AU Tzortziou, M Herman, JR Gallegos, CL Neale, PJ Subramaniam, A Harding, LW Ahmad, Z AF Tzortziou, M Herman, JR Gallegos, CL Neale, PJ Subramaniam, A Harding, LW Ahmad, Z TI Bio-optics of the Chesapeake Bay from measurements and radiative transfer closure SO ESTUARINE COASTAL AND SHELF SCIENCE LA English DT Article DE estuaries; coastal waters; backscattering; chlorophyll fluorescence; particulate absorption; remote sensing ID DISSOLVED ORGANIC-MATTER; INFRARED SPECTRAL REGION; LIGHT-ABSORPTION; COASTAL WATERS; CHLOROPHYLL-A; OCEAN COLOR; AQUATIC PARTICLES; ATLANTIC BIGHT; PHASE FUNCTION; PHYTOPLANKTON AB We combined detailed bio-optical measurements and radiative transfer modeling to perform an 'optical closure' experiment for an optically complex and biologically productive region of the Chesapeake Bay. We used this experiment to evaluate certain assumptions commonly used in bio-optical models, and to investigate which optical characteristics are most important to accurately model and interpret remote sensing ocean-color observations in these Case 2 waters. Direct measurements were made of the magnitude, variability, and spectral characteristics of backscattering and absorption that are critical for accurate parameterizations in satellite bio-optical algorithms and underwater radiative transfer simulations. We found that the ratio of backscattering to total scattering (i.e. the backscattering fraction, b(b)/b) varied considerably depending on particulate loading, distance from land, and mixing processes, and had an average value of 0.0128 at 530 nm. Incorporating information on the magnitude, variability, and spectral characteristics of particulate backscattering into the radiative transfer model, rather than using a volume scattering function commonly assumed for turbid waters, was critical to obtaining agreement between model calculations and measured radiometric quantities. In-situ measurements of absorption coefficients need to be corrected for systematic overestimation due to scattering errors, and this correction commonly employs the assumption that absorption by particulate matter at near-infrared wavelengths is zero. Direct measurements, however, showed that particulate matter in the Bay had small, but non-zero, absorption in the 700-730 nm wavelength region. Accounting for this residual particulate absorption when correcting in-situ measured absorption spectra for scattering errors was important in model simulations of water reflectance in the green wavelengths, where reflectance spectra in estuarine waters peak. Sun-induced chlorophyll fluorescence considerably affected the magnitude of water reflectance in the red wavelengths. Very good optical closure was obtained between independently measured water inherent optical properties and radiation fields, after applying the results from our detailed measurements to model bio-optical processes in these Case 2 waters. The good optical closure was consistent over the observed wide range of water optical characteristics. Average absolute percent differences between measured and model-estimated water-leaving radiances were 6.35% at 443 nm, 7.73% at 554 nm, and 6.86% at 670 nm, considerably smaller than those presented in the few studies of optical closure performed previously in near shore waters of similar optical complexity. These results show that bio-optical processes can be confidently modeled in complex estuarine waters, and underscore the importance of accurate formulations for backscattering, long-wavelength particulate absorption, and chlorophyll fluorescence. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Maryland, Earth Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. Univ Maryland, Horn Point Lab, Ctr Environm Sci, Cambridge, MD 21613 USA. Sci & Data Syst Inc, Silver Spring, MD 20906 USA. RP Tzortziou, M (reprint author), Univ Maryland, Earth Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM martz@code613-3.gsfc.nasa.gov RI Neale, Patrick/A-3683-2012; OI Subramaniam, Ajit/0000-0003-1316-5827; Gallegos, Charles/0000-0001-5112-0166; Herman, Jay/0000-0002-9146-1632 NR 49 TC 64 Z9 71 U1 1 U2 9 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0272-7714 J9 ESTUAR COAST SHELF S JI Estuar. Coast. Shelf Sci. PD JUN PY 2006 VL 68 IS 1-2 BP 348 EP 362 DI 10.1016/j.ecss.2006.02.016 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 057OG UT WOS:000238604500032 ER PT J AU Stanley, JD Jorstad, TF AF Stanley, JD Jorstad, TF TI Short contribution: Buried canopic channel identified near Egypt's Nile Delta Coast with radar (SRTM) imagery SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article ID PATTERNS; POSITION; HISTORY; BRANCH; MOUTH AB Shuttle Radar Topography Mission (SRTM) data, with ground-based geologic investigations, define the geographic position of the relict, Canopic channel in Egypt's NW Nile delta. Two sinuous channel segments south of Abu Qir Bay are observed oil a radar image: a more sinuous trace (36 km in length) west of Idku lagoon, and an eastern one (similar to 20 km), reaching the lagoon's southeast corner. Sediment, cores recovered along channel traces show sand-rich deposits (to > 4 in thick) beneath the surface, in contrast with silty muds in areas away from channels. Historic and archaeological findings indicate that the Ptolemaic Roman city of Schedia once lay directly along the Canopic that channeled water from the 3rd to 2nd centuries B.C. until similar to 5th century A.D., after which Nile water was displaced to the east via Bolbitic and, later, Rosetta branches. Identification of buried, but well-defined, Canopic channels provides baselines for renewed archaeological exploration in this delta sector. (c) 2006 Wiley Periodicals, Inc. C1 Smithsonian Inst, Geoarchaeol Program, Washington, DC 20013 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Geoarchaeol Program, E-205 NMNH, Washington, DC 20013 USA. EM stanleyd@si.edu NR 45 TC 3 Z9 3 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0883-6353 EI 1520-6548 J9 GEOARCHAEOLOGY JI Geoarchaeology PD JUN PY 2006 VL 21 IS 5 BP 503 EP 514 DI 10.1002/gea.20117 PG 12 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA 037CZ UT WOS:000237125600006 ER PT J AU Day, FP Stover, DB Pagel, AL Hungate, BA Dilustro, JJ Herbert, BT Drake, BG Hinkle, CR AF Day, FP Stover, DB Pagel, AL Hungate, BA Dilustro, JJ Herbert, BT Drake, BG Hinkle, CR TI Rapid root closure after fire limits fine root responses to elevated atmospheric CO2 in a scrub oak ecosystem in central Florida, USA SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon dioxide; fine roots; fire; minirhizotrons; root closure; root length ID CARBON-DIOXIDE; ABOVEGROUND BIOMASS; NITROGEN-FIXATION; DYNAMICS; FOREST; DECOMPOSITION; ENRICHMENT; TURNOVER; STORAGE; GROWTH AB Elevated atmospheric carbon dioxide (CO2) often stimulates the growth of fine roots, yet there are few reports of responses of intact root systems to long-term CO2 exposure. We investigated the effects of elevated CO2 on fine root growth using open top chambers in a scrub oak ecosystem at Kennedy Space Center, Florida for more than 7 years. CO2 enrichment began immediately after a controlled burn, which simulated the natural disturbance that occurs in this system every 10-15 years. We hypothesized that (1) root abundance would increase in both treatments as the system recovered from fire; (2) elevated CO2 would stimulate root growth; and (3) elevated CO2 would alter root distribution. Minirhizotron tubes were used to measure fine root length density (mm cm(-2)) every three months. During the first 2 years after fire recovery, fine root abundance increased in all treatments and elevated CO2 significantly enhanced root abundance, causing a maximum stimulation of 181% after 20 months. The CO2 stimulation was initially more pronounced in the top 10 cm and 38-49 cm below the soil surface. However, these responses completely disappeared during the third year of experimental treatment: elevated CO2 had no effect on root abundance or on the depth distribution of fine roots during years 3-7. The results suggest that, within a few years following fire, fine roots in this scrub oak ecosystem reach closure, defined here as a dynamic equilibrium between production and mortality. These results further suggest that elevated CO2 hastens root closure but does not affect maximum root abundance. Limitation of fine root growth by belowground resources - particularly nutrients in this nutrient-poor soil - may explain the transient response to elevated CO2. C1 Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. No Arizona Univ, Dept Sci Biol, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. Savannah River Ecol Lab, Aiken, SC 29802 USA. Virginia Inst Marine Sci, Ctr Coastal Resources Management, Gloucester Point, VA 23062 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. RP Day, FP (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. EM fday@odu.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 45 TC 23 Z9 23 U1 1 U2 14 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JUN PY 2006 VL 12 IS 6 BP 1047 EP 1053 DI 10.1111/j.1365-2486.2006.01148.x PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 043LI UT WOS:000237602200010 ER PT J AU de Santana, CD Crampton, WGR AF David de Santana, Carlos Crampton, William G. R. TI Redescription of the ghost knifefish Apteronotus spurrellii from trans-Andean Colombia (Gymnotiformes : Apteronotidae) SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS LA English DT Article AB We redescribe and provide the first published illustration of Apteronotus spurrellii from the Rio Condoto, a tributary of Rio San Juan on the Pacific slope of Colombia, based on reexamination of the syntypes. This species is diagnosed froth all taxa in the genus Apteronotus sensu stricto by a combination of morphological, morphometric, and meristic characters such as distribution of teeth on the dentary, head length, and numbers of scales above the lateral line at mid-body. C1 Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. Univ Toronto Scarborough, Dept Life Sci, Toronto, ON M1C 1A4, Canada. RP de Santana, CD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, WG-15,MCR 159, Washington, DC 20013 USA. EM apteronotidae@ig.com.br; crampton@utsc.utoronto.ca NR 13 TC 3 Z9 4 U1 0 U2 0 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0936-9902 J9 ICHTHYOL EXPLOR FRES JI Ichthyol. Explor. Freshw. PD JUN PY 2006 VL 17 IS 2 BP 115 EP 120 PG 6 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 050GF UT WOS:000238074800002 ER PT J AU Fuller, NJ AF Fuller, Nancy J. TI The changing face of public history: The Chicago Historical Society and the transformation of an American museum. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Fuller, NJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 2006 VL 93 IS 1 BP 300 EP 301 PG 2 WC History SC History GA 082JL UT WOS:000240382600160 ER PT J AU Ewers, RM Didham, RK AF Ewers, Robert M. Didham, Raphael K. TI Continuous response functions for quantifying the strength of edge effects SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE ecotones; edge effect; edge-effect penetration distance; extent; habitat fragmentation; logistic model; magnitude; patch boundary; scale; unimodal model ID BREEDING BIRD DENSITY; DOUGLAS-FIR FORESTS; HABITAT EDGES; FRAGMENTED LANDSCAPES; VEGETATION RESPONSES; COMMUNITIES; GRADIENTS; GROWTH; CONSERVATION; MAGNITUDE AB 1. Ecological boundaries are a dominant feature of human-modified landscapes and have been the subject of numerous empirical studies. Robust statistical methods for determining the strength of edge effects are a vital requirement for the effective management of species that are negatively affected by habitat boundaries in heavily fragmented landscapes, but development of such methods has been slow. 2. We define edge effects as being composed of two complementary, and statistically definable, components: magnitude (the degree of difference in response values between patch and matrix interiors) and extent (the distance over which the difference in response values can be detected). 3. We present a statistical approach to rigorously delineate edge-effect magnitude and extent. Our approach adapts a form of the general logistic model to describe continuous response functions for any biotic or abiotic variable across ecological boundaries from the landscape matrix into focal patch habitats. The model describes sigmoid and unimodal response functions that have been both theoretically predicted and empirically demonstrated. We use the second derivatives of the functions as an objective means to calculate the magnitude and extent of edge effects, and present a bootstrap technique for calculating confidence intervals around these values. 4. Synthesis and applications. Our results show clearly that edge-effect magnitude and extent are not necessarily correlated, and therefore provide quantitatively different, and complementary, information about the strength of edge effects. Both effect magnitude and extent can be easily used for cross-study comparisons, either by directly comparing the absolute values of response variables in the patch and matrix, or by converting those values to a percentage change. Furthermore, this method provides a management tool for more accurately predicting the presence, spatial location and utilization of core habitat by species in fragmented landscapes. C1 Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand. Smithsonian Trop Res Inst, Balboa, Panama. RP Ewers, RM (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM robert.ewers@ioz.ac.uk RI Didham, Raphael/B-5953-2011 NR 40 TC 96 Z9 103 U1 1 U2 49 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 EI 1365-2664 J9 J APPL ECOL JI J. Appl. Ecol. PD JUN PY 2006 VL 43 IS 3 BP 527 EP 536 DI 10.1111/j.1365-2664.2006.01151.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 042GT UT WOS:000237516600015 ER PT J AU Craig, MT Hastings, PA Pondella, DJ Robertson, DR Rosales-Casian, JA AF Craig, MT Hastings, PA Pondella, DJ Robertson, DR Rosales-Casian, JA TI Phylogeography of the flag cabrilla Epinephelus labriformis (Serranidae): implications for the biogeography of the Tropical Eastern Pacific and the early stages of speciation in a marine shore fish SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Clipperton Atoll; cytochrome b; Epinephelus clippertonensis; Epinephelus labiformis; phylogeography; Serranidae; speciation; species barriers; Tropical Eastern Pacific ID REEF FISHES; GENE FLOW; PELAGIC LARVAE; OCEAN CURRENTS; DNA-SEQUENCES; POPULATION; EVOLUTION; CONSERVATION; MANAGEMENT; DISPERSAL AB Aim To examine the role of previously described biogeographical boundaries in shaping phylogeographical relationships within and among two putative eastern Pacific sibling species, the flag cabrilla, Epinephelus labriformis and the Clipperton grouper, Epinephelus clippertonensis (Serranidae). Location Tropical Eastern Pacific (TEP). Methods Sequence data from the mitochondrial cytochrome b gene were obtained from samples throughout the range of the species. Coalescence analysis, mismatch distributions and an analysis of molecular variance (AMOVA) were used to infer population differentiation. Results Overall, 49 haplotypes were found among 304 specimens, and there was significant structure corresponding to geographical locality (AMOVA, Phi(ct) = 0.198, P < 0.001; Phi(st) = 0.207, P < 0.001; F-st = 0.169, P < 0.001; F-ct = 0.151, P = 0.036). Coalescence analysis indicates a population expansion at Clipperton Atoll during the mid-Pleistocene. Main conclusions Our results suggest that previously described barriers to dispersal along the mainland of the TEP may not impinge on the dispersal ability of marine species, such as these groupers, that have long-lived pelagic larvae. In contrast, gene flow between mainland and island populations of the readily distinguishable morphospecies E. labriformis and E. clippertonensis is restricted. The low level of genetic differentiation between the two species indicates that changes in external colour patterns may evolve more rapidly than genetic markers commonly used to delimit species boundaries. Thus a combination of colour differences and a lack of reciprocal monophyly may act as good indicators of incipient speciation in the marine environment. C1 Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. Occidental Coll, Vantuna Res Grp, Los Angeles, CA 90041 USA. Smithsonian Trop Res Inst, Balboa, Panama. CICESE, Dept Ecol, Ensenada, Baja California, Mexico. RP Craig, MT (reprint author), Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM mtcraig@hawaii.edu NR 65 TC 23 Z9 25 U1 2 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUN PY 2006 VL 33 IS 6 BP 969 EP 979 DI 10.1111/j.1365-2699.2006.01467.x PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 040AX UT WOS:000237352500003 ER PT J AU Niven, JE AF Niven, JE TI Colourful days, colourless nights SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT News Item C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Niven, JE (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM nivenj@si.edu RI Niven, Jeremy/A-5883-2011 NR 1 TC 0 Z9 0 U1 0 U2 1 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD JUN 1 PY 2006 VL 209 IS 11 BP V EP V DI 10.1242/jeb.02284 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 044AF UT WOS:000237643700005 ER PT J AU Morton, ES Howlett, J Kopysh, NC Chiver, I AF Morton, Eugene Sillar Howlett, Joan Kopysh, Nicole Christine Chiver, Ioana TI Song ranging by incubating male Blue-headed Vireos: the importance of song representation in repertoires and implications for song delivery patterns and local/foreign dialect discrimination SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article DE singing style; song dialects; song familiarity; song neighborhood; spatial memory; territorial defense; Vireo solitarius ID BLACK-CAPPED CHICKADEES; WHITE-CROWNED SPARROWS; TIT PARUS-MAJOR; CAROLINA WREN; AUDITORY REPRESENTATION; GEOGRAPHICAL VARIATION; CONSPECIFIC SONGS; UNDEGRADED SONGS; DISTANCE; MEADOWLARKS AB Mechanisms used by birds to rang their distance from singing conspecifics are being debated. In particular, the idea that an incoming song must be in a bird's repertoire for it to be ranged accurately is controversial, but important to our appreciation of the role ranging plays in song evolution. We tested the relation between ranging accuracy and songs in repertoires in playback experiments to male Blue-headed Vireos (Vireo solitarius) whose precise locations were known because they were incubating eggs. Males ranged songs heard while incubating and, when their mates relieved them at the nest, flew directly to the silent playback sites, suggesting that they remembered the locations of simulated intruders. Male vireos approached playback sites of local songs, likely in their own repertoires, more precisely than foreign songs recorded 95-645 km from our study site. Songs included in local and foreign playback tapes differed primarily in frequency modulation, but were similar in other measurements. These results support ranging theory as described by Morton (1986). If the songs within an individual's repertoire are ranged with greater accuracy we discuss how the stability of neighborhoods becomes a factor as to whether or not selection will favor repertoire sharing in song evolution. As well, singing style is affected by ranging. Because Blue-headed Vireos present their songs in a stereotyped order, a listener can compare ordered sequential changes in signal degradation. Comparing degradation in a sequence of songs adds a temporal element that should result in more accurate ranging of the singer's location. C1 Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20008 USA. Univ Guelph, Guelph, ON N1G 2W1, Canada. York Univ, Dept Biol, Toronto, ON M3H 1P3, Canada. RP Morton, ES (reprint author), Hemlock Hill Field Stn, 22318 Teepleville Flats Rd, Cambridge Springs, PA 16403 USA. EM mortone@si.edu NR 55 TC 5 Z9 6 U1 1 U2 12 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD SUM PY 2006 VL 77 IS 3 BP 291 EP 301 DI 10.1111/j.1557-9263.2006.00055.x PG 11 WC Ornithology SC Zoology GA 087GF UT WOS:000240730200008 ER PT J AU Song, J Mathieu, A Soper, RF Popper, AN AF Song, J Mathieu, A Soper, RF Popper, AN TI Structure of the inner ear of bluefin tuna Thunnus thynnus SO JOURNAL OF FISH BIOLOGY LA English DT Article DE hearing; lagena; saccule; sound; tuna; utricle ID HAIR-CELLS; LATERAL-LINE; FISH EAR; HEARING; MORPHOLOGY; SACCULUS; EXPOSURE; LAGENA; STRESS; SOUND AB The ears of five large bluefin tuna Thunnus thynnus were examined by light and scanning electron microscopy (SEM). The gross structure of the ear is similar to that in other fishes. The ears, however, appear to be held more rigidly in place than in other species through the presence of an extensive connective tissue between the membranous ear and the surrounding bone. Moreover, unlike other fishes, the semicircular canals and otolithic end organs have thick cartilaginous walls and there is a dense matrix surrounding the otoliths rather than a more watery fluid found in other species. SEM revealed that the saccular epithelium has a 'standard' hair cell orientation pattern. The hair cell orientation patterns in the lagena and utricle resemble those found in most other fishes. Ciliary bundle density and length vary in different epithelial regions and each ear had > 2 x 10(6) sensory cells. The morphological results support the hypothesis that bluefin tuna probably do not detect sounds to much over 1000 Hz (if that high) and that only very loud anthropogenic sounds have the potential to affect hearing in this species. (c) 2006 The Fisheries Society of the British Isles. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. Univ Maryland, Ctr Comparat & Evolutionary Biol Hearing, College Pk, MD 20742 USA. Oceans Ltd, St John, NF A1C 2H1, Canada. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. RP Popper, AN (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM Apopper@umd.edu NR 28 TC 10 Z9 12 U1 4 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD JUN PY 2006 VL 68 IS 6 BP 1767 EP 1781 DI 10.1111/j.1095-8649.2006.01057.x PG 15 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 058FY UT WOS:000238652100011 ER PT J AU Graves, GR AF Graves, Gary R. TI Possible predation of great gray owl by a barred owl SO JOURNAL OF RAPTOR RESEARCH LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. Univ Minnesota, Dept Biol, Duluth, MN 55811 USA. Univ Minnesota, Nat Resources Res Inst, Ctr Water & Environm, Duluth, MN 55811 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC-116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu NR 0 TC 2 Z9 2 U1 1 U2 4 PU RAPTOR RESEARCH FOUNDATION INC PI HASTINGS PA 14377 117TH STREET SOUTH, HASTINGS, MN 55033 USA SN 0892-1016 J9 J RAPTOR RES JI J. Raptor Res. PD JUN PY 2006 VL 40 IS 2 BP 175 EP 175 DI 10.3356/0892-1016(2006)40[175:PPOGGO]2.0.CO;2 PG 1 WC Ornithology SC Zoology GA 082JQ UT WOS:000240383200013 ER PT J AU Rueda, LM Kim, HC Klein, TA Pecor, JE Li, C Sithiprasasna, R Debboun, M Wilkerson, RC AF Rueda, Leopoldo M. Kim, Heung-Cheul Klein, Terry A. Pecor, James E. Li, Cong Sithiprasasna, Ratana Debboun, Mustapha Wilkerson, Richard C. TI Distribution and larval habitat characteristics of Anopheles Hyrcanus Group and related mosquito species (Diptera : Culicidae) in South Korea SO JOURNAL OF VECTOR ECOLOGY LA English DT Article DE mosquitoes; Anopheles; Hyrcanus Group; malaria; Diptera; Culicidae; Korea ID SINENSIS; MALARIA; VECTOR C1 Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Supprt Ctr, Suitland, MD 20746 USA. USA, Med Detachment 5, Med Command 18, Unit 15247, APO, AP 96205 USA. USA, Force Hlth Protect, Med Command 18, Unit 15281, APO, AP 96205 USA. Armed Forces Res Inst Med Sci, Dept Entomol, USA Med Component, Bangkok, Thailand. USA, Med Dept Ctr & Sch, Acad Hlth Sci, Med Zool Branch, Ft Sam Houston, TX 78234 USA. RP Rueda, LM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Supprt Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. RI Valle, Ruben/A-7512-2013 NR 27 TC 16 Z9 18 U1 1 U2 2 PU SOC VECTOR ECOLOGY PI CORONA PA 1966 COMPTON AVE, CORONA, CA 92881 USA SN 1081-1710 EI 1948-7134 J9 J VECTOR ECOL JI J. Vector Ecol. PD JUN PY 2006 VL 31 IS 1 BP 198 EP 205 DI 10.3376/1081-1710(2006)31[198:DALHCO]2.0.CO;2 PG 8 WC Entomology SC Entomology GA 062HX UT WOS:000238936300027 PM 16859110 ER PT J AU Laube, S Zotz, G AF Laube, Stefan Zotz, Gerhard TI Long-term changes of the vascular epiphyte assemblage on the palm Socratea exorrhiza in a lowland forest in Panama SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE community stability; dispersal limitation; host tree; mortality ID HUMID MONTANE FOREST; TROPICAL FOREST; POPULATION-DYNAMICS; COSTA-RICA; VEGETATION; COLONIZATION; GRADIENT; ECOLOGY; GROWTH; ORCHID AB Question: What are the qualitative and quantitative long-term changes in the vascular epiphyte assemblage on a particular host tree species? Location: Lowland rain forest of the San Lorenzo Crane Plot, Republic of Panama. Methods: We followed the fate of the vascular epiphyte assemblage on 99 individuals of the palm Socratea exorrhiza by three censuses over the course of five years. Results: The composition of the epiphyte assemblage changed little during the course of the study. While the similarity of epiphyte vegetation decreased on individual palms through time, the similarity analysed over all palms increased Even well established epiphyte individuals experienced high mortality with only 46% of the originally mapped individuals surviving the following five years. We found a positive correlation between host tree size and epiphyte richness and detected higher colonization rates of epiphytes per surface area on larger trees. Conclusions: Epiphyte assemblages on individual S. exorrhiza trees were highly dynamic while the overall composition of the epiphyte vegetation on the host tree species in the study plot was stable. We suggest that higher recruitment rates, due to localized seed dispersal by already established epiphytes, on larger palms promote the colonization of epiphytes on larger palms. Given the known growth rates and mortality rates of the host tree species, the maximum time available for colonization and reproduction of epiphytes on a given tree is estimated to be ca. 60 years. This time frame will probably be too short to allow assemblages to be ever saturated. C1 Univ Kaiserslautern, D-67653 Kaiserslautern, Germany. Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Laube, S (reprint author), Univ Kaiserslautern, D-67653 Kaiserslautern, Germany. EM s.laube@web.de NR 37 TC 15 Z9 17 U1 3 U2 14 PU OPULUS PRESS UPPSALA AB PI GRANGARDE PA GAMLA VAGEN 40, S-770 13 GRANGARDE, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD JUN PY 2006 VL 17 IS 3 BP 307 EP 314 DI 10.1111/j.1654-1103.2006.tb02450.x PG 8 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 071FZ UT WOS:000239585700006 ER PT J AU Baitchman, EJ Calle, PP Clippinger, TL Deem, SL James, SB Raphael, BL Cook, RA AF Baitchman, EJ Calle, PP Clippinger, TL Deem, SL James, SB Raphael, BL Cook, RA TI Preliminary evaluation of blood lipid profiles in captive western lowland gorillas (Gorilla gorilla gorilla) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Gorilla gorilla gorilla; cholesterol; lipids; lipoprotein; apolipoprotein; atherosclerosis ID CORONARY HEART-DISEASE; HDL-CHOLESTEROL AB Published serum cholesterol values in captive western lowland gorillas (Gorilla gorilla gorilla) are much higher than human ranges, with a national mean of 7.36 mmol/L (284 mg/dl, n = 863). Complete blood lipid profiles were examined in 15 captive gorillas. High-density lipoprotein (HDL) was found to decrease more rapidly with age than total cholesterol, resulting in an increasing ratio of cholesterol HDL with age. The ratio of apolipoprotein B to apolipoprotein A1 also increased with age. Establishment of a database of blood lipid values for captive gorillas with correlative analysis of animals with known atherosclerosis status may help to identify sensitive predictors of coronary heart disease risk. C1 Zoo New England, Boston, MA 02121 USA. Wildlife Conservat Soc, Dept Clin Care, Bronx, NY 10460 USA. Zool Soc San Diego, San Diego Zoo, San Diego, CA 92112 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Baitchman, EJ (reprint author), Zoo New England, 1 Franklin Pk Rd, Boston, MA 02121 USA. NR 15 TC 3 Z9 4 U1 0 U2 6 PU AMER ASSOC ZOO VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 2006 VL 37 IS 2 BP 126 EP 129 DI 10.1638/05-064.1 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 051XW UT WOS:000238196000005 PM 17312789 ER PT J AU Riley, S AF Riley, S TI The Cinderella pact. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC 20560 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 JUN 1 PY 2006 VL 131 IS 10 BP 113 EP 114 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 051ED UT WOS:000238142800101 ER PT J AU Aiello, A AF Aiello, A TI A walk around the pond: Insects in and over the water. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. 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 JUN 1 PY 2006 VL 131 IS 10 BP 150 EP 150 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 051ED UT WOS:000238142800237 ER PT J AU Kline, DI Bryant, J Kisflaudy, E Rohwer, G Nostropaur, F Grayson, J Knowlton, N Rohwer, F AF Kline, David I. Bryant, John Kisflaudy, Eddie Rohwer, Gary Nostropaur, Fernando Grayson, Jodi Knowlton, Nancy Rohwer, Forest TI The aquatic automated dosing and maintenance system (AADAMS) SO LIMNOLOGY AND OCEANOGRAPHY-METHODS LA English DT Article ID CORAL PORITES-CYLINDRICA; STYLOPHORA-PISTILLATA; SCLERACTINIAN CORAL; NITRATE ENRICHMENT; MULTIPLE STRESSORS; ORGANIC-CARBON; PHOTOSYNTHESIS; TEMPERATURE; METABOLISM; COPPER AB The maintenance and dosing of aquatic organisms, such as corals and mollusks, are essential for ecotoxicology studies, yet it is difficult to maintain many of these sensitive organisms for an extended period. Consequently, many previous aquatic ecotoxicology experiments have been limited in their number of replicates and maintained in one or a few experimental aquaria, with only a limited number of stressors tested in each experiment. Here we describe a modular system that overcomes many of the difficulties of maintaining large numbers of sensitive aquatic organisms in separate containers, and allows testing of a large suite of stressors in each experiment. The AADAMS (aquatic automated dosing and maintenance system) allows testing of 40 independent stressors with 10 independent replicates per stressor (400 individuals total). The AADAMS provides surge and regular water changes simultaneously with accurate dosing via Venturi valves. In a series of experiments over a 1-year period, the AADAMS was used to test the effects of various factors affecting water quality on Caribbean coral reefs. Roofing tar and road asphalt were two of the most damaging pollutants tested, with LD50 values (lethal dose that killed 50% of the corals) of 0.013 g L-1 and 0.079 g L-1, respectively, thus suggesting that runoff from roads and near-shore construction could be contributing to reef decline. The AADAMS is an accurate, reliable system for highly replicated ecotoxicological studies of sensitive aquatic organisms, which are important indicators of ecosystem health. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodiverst & Conservat, La Jolla, CA 92093 USA. San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. Teqcom Ind, Santa Ana, CA USA. Bar Diamond Inc, Parma, ID USA. Univ Calif San Diego, Scripps Inst Oceanog, Birch Aquarium Scripps, La Jolla, CA 92093 USA. J Grayson Biol Consulting, Bamfield, BC, Canada. San Diego State Univ, Ctr Microbial Sci, San Diego, CA 92182 USA. RP Kline, DI (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. NR 35 TC 1 Z9 1 U1 0 U2 4 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA J9 LIMNOL OCEANOGR-METH JI Limnol. Oceanogr. Meth. PD JUN PY 2006 VL 4 BP 184 EP 192 PG 9 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 070AQ UT WOS:000239493100003 ER PT J AU Maldonado, JE Leonard, J Miranda, GA Ortega, J Wayne, RK Aguilera, RJ AF Maldonado, Jesus E. Leonard, Jennifer Miranda, Gustavo A. Ortega, Jorge Wayne, Robert K. Aguilera, Renato J. TI Ten polymorphic microsatellite loci for the endangered Buena Vista Lake shrew (Sorex ornatus relictus) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE microsatellite; ornate shrew; primer; Sorex ornatus relictus; Soricidae AB The ornate shrew (Sorex ornatus) is restricted to the vanishing wetlands of California, USA and Baja California, Mexico. Several subspecies of ornate shrews are considered 'mammal species of special concern' in California by the Department of Fish and Game, and one (Sorex ornatus relictus) has recently been listed as endangered. Populations of shrews around Buena Vista Lake have been diminished or extirpated due to habitat deterioration and human development. In order to study the patterns of genetic variation in isolated populations of Buena Vista Lake shrews, we developed 10 polymorphic microsatellite loci. There were 6-27 alleles per locus, and the loci had heterozygosity values that ranged from 20 to 80%. In addition, we screened 20 different populations of S. ornatus, eight species within two subfamilies of shrews (Soricinae and Crocidurinae), as well as in a mole (Talpidae, Neurotrichus gibbsii), to determine if these loci could be informative in other species as well. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Dept Mol Cellular & Dev Biol, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, David Geffen Sch Med, Los Angeles, CA 90095 USA. Univ Nacl Autonoma Mexico, Inst Ecol, Lab Macroecol, Mexico City, DF, Mexico. Univ Texas, Dept Sci Biol, El Paso, TX 79968 USA. RP Ortega, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM artibeus2@aol.com RI Leonard, Jennifer/A-7894-2010 OI Leonard, Jennifer/0000-0003-0291-7819 NR 9 TC 2 Z9 3 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD JUN PY 2006 VL 6 IS 2 BP 349 EP 352 DI 10.1111/j.1471-8286.2005.01228.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 043XJ UT WOS:000237635900017 ER PT J AU Schulte, JA Macey, JR Papenfuss, TJ AF Schulte, JA Macey, JR Papenfuss, TJ TI A genetic perspective on the geographic association of taxa among and North American lizards of the Sceloporus magister complex (Squamata : Iguanidae : Phrynosomatinae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID TRANSFER-RNA GENES; PHYLOGENETIC-RELATIONSHIPS; HISTORICAL BIOGEOGRAPHY; MOLECULAR PHYLOGENETICS; SPECIES GROUP; MITOCHONDRIAL GENOME; MORPHOLOGICAL DATA; CONFIDENCE-LIMITS; EVOLUTION; DNA C1 Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. Lawrence Berkeley Natl Lab, Joint Genome Inst, Dept Evolut Genom, Walnut Creek, CA 94598 USA. Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Schulte, JA (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, POB 37012,MRC 162, Washington, DC 20013 USA. EM Schulte.James@nmnh.si.edu NR 44 TC 10 Z9 11 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 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUN PY 2006 VL 39 IS 3 BP 873 EP 880 DI 10.1016/j.ympev.2005.04.033 PG 8 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 051IR UT WOS:000238155300021 PM 16580231 ER PT J AU Erdogdu, P Huchra, JP Lahav, O Colless, M Cutri, RM Falco, E George, T Jarrett, T Jones, DH Kochanek, CS Macri, L Mader, J Martimbeau, N Pahre, M Parker, Q Rassat, A Saunders, W AF Erdogdu, P. Huchra, J. P. Lahav, O. Colless, M. Cutri, R. M. Falco, E. George, T. Jarrett, T. Jones, D. H. Kochanek, C. S. Macri, L. Mader, J. Martimbeau, N. Pahre, M. Parker, Q. Rassat, A. Saunders, W. TI The dipole anisotropy of the 2 micron all-sky redshift survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; Local Group; cosmology : observations; large-scale structure of Universe; infrared : galaxies ID SPHERICAL HARMONIC-ANALYSIS; LARGE-SCALE STRUCTURE; LOCAL GROUP; BACKGROUND-RADIATION; IRAS GALAXIES; DARK-MATTER; VELOCITY-FIELD; TULLY-FISHER; REAL-SPACE; MILKY-WAY AB We estimate the acceleration on the Local Group (LG) from the 2 Micron All-Sky Redshift Survey (2MRS). The sample used includes about 23 200 galaxies with extinction-corrected magnitudes brighter than K(s)= 11.25 and it allows us to calculate the flux-weighted dipole. The near-infrared flux-weighted dipoles are very robust because they closely approximate a mass-weighted dipole, bypassing the effects of redshift distortions and require no preferred reference frame. This is combined with the redshift information to determine the change in dipole with distance. The misalignment angle between the LG and the cosmic microwave background (CMB) dipole drops to 12 degrees +/- 7 degrees at around 50 h(-1) Mpc, but then increases at larger distances, reaching 21 degrees +/- 8 degrees at around 130 h(-1) Mpc. Exclusion of the galaxies Maffei 1, Maffei 2, Dwingeloo 1, IC342 and M87 brings the resultant flux dipole to 14 degrees +/- 7 degrees away from the CMB velocity dipole. In both cases, the dipole seemingly converges by 60 h(-1) Mpc. Assuming convergence, the comparison of the 2MRS flux dipole and the CMB dipole provides a value for the combination of the mass density and luminosity bias parameters Omega(0.6)(m)/b(L)= 0.40 +/- 0.09. C1 Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey. Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. Anglo Australian Observ, Epping, NSW 2052, Australia. CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. CALTECH, Pasadena, CA 91109 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43221 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. WM Keck Observ, Kamuela, HI 96743 USA. Macquarie Univ, Dept Phys, Sydney, NSW 2109, Australia. Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Erdogdu, P (reprint author), Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey. EM Pirin.Erdogdu@nottingham.ac.uk OI Rassat, Anais/0000-0002-5476-6461; Colless, Matthew/0000-0001-9552-8075; Macri, Lucas/0000-0002-1775-4859 NR 68 TC 69 Z9 69 U1 0 U2 3 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 JUN 1 PY 2006 VL 368 IS 4 BP 1515 EP 1526 DI 10.1111/j.1365-2966.2006.10243.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046LI UT WOS:000237812700004 ER PT J AU Soria, R Fender, RP Hannikainen, DC Read, AM Stevens, IR AF Soria, R. Fender, R. P. Hannikainen, D. C. Read, A. M. Stevens, I. R. TI An ultraluminous X-ray microquasar in NGC 5408 ? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; supernova remnants; radio continuum : ISM; X-rays : binaries; X-rays : individual : NGC 5408 X-1 ID ACTIVE GALACTIC NUCLEI; ACCRETING BLACK-HOLE; SD GALAXY NGC-300; RADIO-SOURCES; SUPERNOVA-REMNANTS; RELATIVISTIC JETS; MAGELLANIC CLOUDS; LOW/HARD STATE; HII-REGIONS; HOLMBERG-II AB We studied the radio source associated with the ultraluminous X-ray source in NGC 5408 (L(X) approximate to 10(40) erg s(-1)). The radio spectrum is steep (index approximate to -1), consistent with optically thin synchrotron emission, not with flat-spectrum core emission. Its flux density (approximate to 0.28 mJy at 4.8 GHz, at a distance of 4.8 Mpc) was the same in the March 2000 and December 2004 observations, suggesting steady emission rather than a transient outburst. However, it is orders of magnitude higher than expected from steady jets in stellar-mass microquasar. Based on its radio flux and spectral index, we suggest that the radio source is either an unusually bright supernova remnant, or, more likely, a radio lobe powered by a jet from the black hole (BH). Moreover, there is speculative evidence that the source is marginally resolved with a radius similar to 30 pc. A faint H II region of similar size appears to coincide with the radio and X-ray sources, but its ionization mechanism remains unclear. Using a self-similar solution for the expansion of a jet-powered electron-positron plasma bubble, in the minimum-energy approximation, we show that the observed flux and (speculative) size are consistent with an average jet power approximate to 7 x 10(38) erg s(-1)similar to 0.1L(X) similar to 0.1L(Edd), an age approximate to 10(5) yr, a current velocity of expansion approximate to 80 km s(-1). We briefly discuss the importance of this source as a key to understand the balance between luminosity and jet power in accreting BHs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Helsinki, FIN-00014 Helsinki, Finland. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Soria, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rsoria@cfa.harvard.edu NR 96 TC 33 Z9 33 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 JUN 1 PY 2006 VL 368 IS 4 BP 1527 EP 1539 DI 10.1111/j.1365-2966.2006.10250.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046LI UT WOS:000237812700005 ER PT J AU McKinney, JC AF McKinney, Jonathan C. TI General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE accretion, accretion discs; black hole physics; galaxies : jets; gamma-rays : bursts; X-rays : bursts ID GAMMA-RAY BURSTS; ACTIVE GALACTIC NUCLEI; MAGNETICALLY DRIVEN ACCRETION; MAGNETIZED NEUTRON-STARS; BLANDFORD-ZNAJEK PROCESS; DOUBLE RADIO-SOURCES; 29 MARCH 2003; CORE-COLLAPSE; POYNTING FLUX; X-RAY AB The formation and large-scale propagation of Poynting-dominated jets produced by accreting, rapidly rotating black hole systems are studied by numerically integrating the general relativistic magnetohydrodynamic equations of motion to follow the self-consistent interaction between accretion discs and black holes. This study extends previous similar work by studying jets till t approximate to 10(4)GM/c(3) out to r approximate to 10(4)GM/c(2), by which the jet is superfast magnetosonic and moves at a lab-frame bulk Lorentz factor of Gamma similar to 10 with a maximum terminal Lorentz factor of Gamma(infinity)less than or similar to 10(3). The radial structure of the Poynting-dominated jet is piece-wise self-similar, and fits to flow quantities along the field line are provided. Beyond the Alfven surface at r similar to 10-100GM/c(2), the jet becomes marginally unstable to (at least) current-driven instabilities. Such instabilities drive shocks in the jet that limit the efficiency of magnetic acceleration and collimation. These instabilities also induce jet substructure with 3 less than or similar to Gamma less than or similar to 15. The jet is shown to only marginally satisfy the necessary and sufficient conditions for kink instability, so this may explain how astrophysical jets can extend to large distances without completely disrupting. At large distance, the jet angular structure is Gaussian-like (or uniform within the core with sharp exponential wings) with a half-opening angle of approximate to 5 degrees and there is an extended component out to approximate to 27 degrees. Unlike in some hydrodynamic simulations, the environment is found to play a negligible role in jet structure, acceleration, and collimation as long as the ambient pressure of the surrounding medium is small compared to the magnetic pressure in the jet. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP McKinney, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM jmckinney@cfa.harvard.edu NR 218 TC 286 Z9 286 U1 0 U2 7 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 JUN 1 PY 2006 VL 368 IS 4 BP 1561 EP 1582 DI 10.1111/j.1365-2966.2006.10256.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046LI UT WOS:000237812700007 ER PT J AU Ascasibar, Y Jean, P Boehm, C Knodlseder, J AF Ascasibar, Y. Jean, P. Boehm, C. Knodlseder, J. TI Constraints on dark matter and the shape of the Milky Way dark halo from the 511-keV line SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy : halo; dark matter ID POSITRON-ANNIHILATION RADIATION; GALAXY ROTATION CURVES; GALACTIC-CENTER REGION; N-BODY SIMULATIONS; LAMBDA-CDM HALOES; DENSITY PROFILES; INNER STRUCTURE; NEUTRINO SCATTERING; FINE-STRUCTURE; MASS PROFILES AB About one year ago, it was speculated that decaying or annihilating light dark matter (LDM) particles could explain the flux and extension of the 511-keV line emission in the Galactic Centre. Here, we present a thorough comparison between theoretical expectations of the Galactic positron distribution within the LDM scenario and observational data from INTEGRAL/SPI. Unlike previous analyses, there is now enough statistical evidence to put tight constraints on the shape of the dark matter (DM) halo of our Galaxy, if the Galactic positrons originate from DM. For annihilating candidates, the best fit to the observed 511-keV emission is provided by a radial density profile with inner logarithmic slope gamma= 1.03 +/- 0.04. In contrast, decaying DM requires a much steeper density profile, gamma > 1.5, rather disfavoured by both observations and numerical simulations. Within the annihilating LDM scenario, a velocity-independent cross-section would be consistent with the observational data while a cross-section purely proportional to v(2) can be rejected at a high confidence level. Assuming the most simplistic model where the Galactic positrons are produced as primaries, we show that the LDM candidate should be a scalar rather than a spin-1/2 particle and obtain a very stringent constraint on the value of the positron production cross-section to explain the 511-keV emission. One consequence is that the value of the fine structure constant alpha should differ from that recommended in the CODATA (Committee on Data for Science and Technology). This is a very strong test for the LDM scenario and an additional motivation in favour of experiments measuring alpha directly. Our results finally indicate that an accurate measurement of the shape of the dark halo profile could have a tremendous impact on the determination of the origin of the 511-keV line and vice versa. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Univ Toulouse 3, F-31062 Toulouse, France. CERN, Div Theory, Dept Phys, CH-1211 Geneva 23, Switzerland. RP Ascasibar, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yago@head.cfa.harvard.edu OI Ascasibar Sequeiros, Yago/0000-0003-1577-2479 NR 62 TC 61 Z9 61 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2006 VL 368 IS 4 BP 1695 EP 1705 DI 10.1111/j.1365-2966.2006.10226.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046LI UT WOS:000237812700015 ER PT J AU Jonker, PG Bassa, CG Nelemans, G Juett, AM Brown, EF Chakrabarty, D AF Jonker, PG Bassa, CG Nelemans, G Juett, AM Brown, EF Chakrabarty, D TI The neutron star soft X-ray transient 1H 1905+000 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : general; stars : individual; 1H 1905+000; stars : neutron; X-rays : binaries ID XMM-NEWTON OBSERVATIONS; BLACK-HOLE; LOW-MASS; CHANDRA OBSERVATIONS; THERMAL EMISSION; SAX J1808.4-3658; BINARIES; BURSTS; EQUILIBRIUM; KS-1731-260 AB In this paper, we report on our analysis of a similar to 25 ks. Chandra X-ray observation of the neutron star soft X-ray transient (SXT) 1H 1905+000 in quiescence. Furthermore, we discuss our findings of the analysis of optical photometric observations which we obtained using the Magellan telescope and photometric and spectroscopic observations which we obtained using the Very Large Telescope (VLT) at Paranal. The X-ray counterpart of 1H 1905+000 was not detected in our Chandra data, with a 95 per cent confidence limit to the source count rate of 1.2 x 10(-4) counts s(-1). For different spectral models this yields an upper limit on the luminosity of 1.8 x 10(31) erg s(-1) (for an upper limit on the distance of 10 kpc). This luminosity limit makes 1H 1905+000 the faintest neutron star SXT in quiescence observed to date. The neutron star luminosity is so low that it is similar to the lowest luminosities derived for black hole (BH) SXTs in quiescence. This low luminosity for a neutron star SXT challenges the hypothesis presented in the literature that BH SXTs in quiescence have lower luminosities than neutron star SXTs as a result of the presence of a BH event horizon. Furthermore, the limit on the neutron star luminosity obtained less than 20 yr after the outburst has ceased, constrains the thermal conductivity of the neutron star crust. Finally, the neutron star core must be so cold that unless the time-averaged mass accretion rate is lower than 2 x 10(-12) M-circle dot yr(-1), core cooling has to proceed via enhanced neutrino emission processes. The time-averaged mass accretion rate can be derived from binary evolution models if the orbital period of the system is known. Our optical observations show that the optical counterpart discovered when the source was in outburst has faded. Near the outburst optical position we find two stars with a separation of 0.7 arcsec and I= 19.3 +/- 0.1 and 21.3 +/- 0.1. VLT optical spectroscopy revealed that the spectrum of the brighter of the two sources is a G5-7V star. However, the outburst astrometric position of the optical counterpart does not coincide with the position of the G5-7V star nor with that of the fainter star. We derive a limit on the absolute I-band magnitude of the quiescent counterpart of M-I > 7.8 assuming the source is at 10 kpc. This is in line with 1H 1905+000 being an ultracompact X-ray binary, as has been proposed based on the low-outburst V-band absolute magnitude. C1 SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Inst Astron, NL-3508 TA Utrecht, Netherlands. Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Jonker, PG (reprint author), SRON, Natl Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Brown, Edward/F-1721-2011; Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 NR 66 TC 28 Z9 28 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2006 VL 368 IS 4 BP 1803 EP 1810 DI 10.1111/j.1365-2966.2006.10253.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 046LI UT WOS:000237812700026 ER PT J AU Olendorf, R Rodd, FH Punzalan, D Houde, AE Hurt, C Reznick, DN Hughes, KA AF Olendorf, R Rodd, FH Punzalan, D Houde, AE Hurt, C Reznick, DN Hughes, KA TI Frequency-dependent survival in natural guppy populations SO NATURE LA English DT Article ID RETICULATA-PETERS PISCES; LIFE-HISTORY EVOLUTION; POECILIA-RETICULATA; SEXUAL SELECTION; FEMALE CHOICE; COLOR POLYMORPHISM; MATE PREFERENCE; MALE TRAITS; PREDATION; PATTERNS AB The maintenance of genetic variation in traits under natural selection is a long-standing paradox in evolutionary biology(1-3). Of the processes capable of maintaining variation, negative frequency-dependent selection ( where rare types are favoured by selection) is the most powerful, at least in theory(1); however, few experimental studies have confirmed that this process operates in nature. One of the most extreme, unexplained genetic polymorphisms is seen in the colour patterns of male guppies ( Poecilia reticulata)(4,5). Here we manipulated the frequencies of males with different colour patterns in three natural populations to estimate survival rates, and found that rare phenotypes had a highly significant survival advantage compared to common phenotypes. Evidence from humans(6,7) and other species(8,9) implicates frequency-dependent survival in the maintenance of molecular, morphological and health-related polymorphisms. As a controlled manipulation in nature, this study provides unequivocal support for frequency-dependent survival - an evolutionary process capable of maintaining extreme polymorphism. C1 Univ Illinois, Sch Integrat Biol, Urbana, IL 61801 USA. Univ Illinois, Inst Genome Biol, Urbana, IL 61801 USA. Univ Toronto, Dept Zool, Toronto, ON M5S 3G5, Canada. Lake Forest Coll, Dept Biol, Lake Forest, IL 60045 USA. Naos Marine Lab, Smithsonian Trop Res Inst, Panama City, Panama. Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. RP Hughes, KA (reprint author), Univ Illinois, Sch Integrat Biol, Urbana, IL 61801 USA. EM kahughes@life.uiuc.edu RI Hurt, Carla/A-3284-2011 NR 29 TC 118 Z9 124 U1 17 U2 119 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 1 PY 2006 VL 441 IS 7093 BP 633 EP 636 DI 10.1038/nature04646 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 048AU UT WOS:000237920800047 PM 16738659 ER PT J AU Szentgyorgyi, A AF Szentgyorgyi, Andrew TI Hectochelle: High resolution multiobject spectroscopy at the MMT SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT Conference on Integral Field Spectroscopy CY JUL 04-08, 2005 CL Durham, ENGLAND DE instrumentation; spectrographs; techniques; spectroscopic methods ID SPECTROGRAPH; HECTOSPEC AB Hectochelle is a optical fiber-fed echelle spectrograph commissioned at the MMT in early 2004 with 240 fibers. Hectochelle is a single order echelle where each order is similar to 150 angstrom and has a resolution of similar to 34,000. The usable passband of the Hectochelle is 3800-9000 angstrom. (c) 2006 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Szentgyorgyi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM saint@cfa.harvard.edu NR 3 TC 6 Z9 6 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD JUN PY 2006 VL 50 IS 4-5 BP 326 EP 328 DI 10.1016/j.newar.2006.02.002 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 061QT UT WOS:000238888200020 ER PT J AU Engelbrecht, BMJ Dalling, JW Pearson, TRH Wolf, RL Galvez, DA Koehler, T Tyree, MT Kursar, TA AF Engelbrecht, BMJ Dalling, JW Pearson, TRH Wolf, RL Galvez, DA Koehler, T Tyree, MT Kursar, TA TI Short dry spells in the wet season increase mortality of tropical pioneer seedlings SO OECOLOGIA LA English DT Article DE BCI; diversity; drought; gap partitioning; survival ID RAIN-FOREST; SEED SIZE; NEOTROPICAL PIONEERS; TREE SEEDLINGS; MOIST FOREST; SPECIES RICHNESS; GROWTH-RESPONSES; GAP SIZE; DROUGHT; SURVIVAL AB Variation in plant species performance in response to water availability offers a potential axis for temporal and spatial habitat partitioning and may therefore affect community composition in tropical forests. We hypothesized that short dry spells during the wet season are a significant source of mortality for the newly emerging seedlings of pioneer species that recruit in treefall gaps in tropical forests. An analysis of a 49-year rainfall record for three forests across a rainfall gradient in central Panama confirmed that dry spells of >= 10 days during the wet season occur on average once a year in a deciduous forest, and once every other year in a semi-deciduous moist and an evergreen wet forest. The effect of wet season dry spells on the recruitment of pioneers was investigated by comparing seedling survival in rain-protected dry plots and irrigated control plots in four large artificially created treefall gaps in a semi-deciduous tropical forest. In rain-protected plots surface soil layers dried rapidly, leading to a strong gradient in water potential within the upper 10 cm of soil. Seedling survival for six pioneer species was significantly lower in rain-protected than in irrigated control plots after only 4 days. The strength of the irrigation effect differed among species, and first became apparent 3-10 days after treatments started. Root allocation patterns were significantly, or marginally significantly, different between species and between two groups of larger and smaller seeded species. However, they were not correlated with seedling drought sensitivity, suggesting allocation is not a key trait for drought sensitivity in pioneer seedlings. Our data provide strong evidence that short dry spells in the wet season differentially affect seedling survivorship of pioneer species, and may therefore have important implications to seedling demography and community dynamics. C1 Smithsonian Trop Res Inst, Panama City, Panama. Tech Univ Kaiserlautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. US Forest Serv, USDA, Burlington, VT 05402 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Panama City, Panama. EM engelbrb@bci.si.edu RI Engelbrecht, Bettina/E-9914-2012 NR 53 TC 59 Z9 60 U1 0 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2006 VL 148 IS 2 BP 258 EP 269 DI 10.1007/s00442-006-0368-5 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 055BR UT WOS:000238425500009 PM 16514537 ER PT J AU Hu, XS He, FL Hubbell, SP AF Hu, Xin-Sheng He, Fangliang Hubbell, Stephen P. TI Neutral theory in macroecology and population genetics SO OIKOS LA English DT Article ID SPECIES ABUNDANCE; COMMUNITY STRUCTURE; TROPICAL FORESTS; SAMPLING THEORY; BETA-DIVERSITY; DRIFT MODEL; BIODIVERSITY; ECOLOGY; COMPETITION; DISPERSAL AB Current neutral theory in macroecology has many parallels with neutral theory in population genetics, but it also has many distinct features that arise because it focuses mainly on questions at the community level rather than at the population level. Here we highlight the similarities and differences between these two bodies of theories from the aspects of the operational units, definitions of neutrality, basic parameters, driving forces, spatial structure and community assembly rules. Compared with neutral theory in population genetics, whose development spans more than 40 years, neutral theory in ecology, which is only a few years old, is still immature and under-developed. There are many opportunities for major theoretical contributions, some of which can be adopted directly from population genetics, while others will require new theoretical work. We critically discuss these opportunities and theoretical challenges in neutral macroecology, particularly in regard to effective community size, ecological drift, community differentiation and ecological dominance. C1 Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. 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 NR 55 TC 49 Z9 54 U1 2 U2 37 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0030-1299 J9 OIKOS JI Oikos PD JUN PY 2006 VL 113 IS 3 BP 548 EP 556 DI 10.1111/j.2006.0030-1299.14837.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 050QU UT WOS:000238103800017 ER PT J AU Vanne, YV Saenz, A Dalgarno, A Forrey, RC Froelich, P Jonsell, S AF Vanne, YV Saenz, A Dalgarno, A Forrey, RC Froelich, P Jonsell, S TI Doubly excited autoionizing states of H-2 converging to the H(n=2)+H(n '=2) limit SO PHYSICAL REVIEW A LA English DT Article ID IONIZATION AB A numerical investigation of the doubly excited states of H-2 converging to the H(n=2)+H(n'=2) limit was performed. Special emphasis was put on the accurate description of the range of intermediate internuclear distances in order to correctly connect the short range with the asymptotic van der Waals regime where perturbation theory is applicable. The present nonperturbative calculation extends to internuclear separations R=200a(0) and is sufficiently accurate to achieve a connection between the two extreme regimes without any need for an interpolation procedure. The high precision of the ab initio results revealed a long range dipole-quadrupole interaction that had been omitted in two earlier calculations. In addition to revised first-order perturbation theory results the leading second-order term varying as R-6 was obtained. The impact of the present findings for cold H(n=2) collisions is briefly discussed. C1 Humboldt Univ, AG Moderne Opt, Inst Phys, D-10117 Berlin, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA. Univ Uppsala, Dept Quantum Chem, S-75120 Uppsala, Sweden. Umea Univ, Dept Phys, S-90187 Umea, Sweden. RP Vanne, YV (reprint author), Humboldt Univ, AG Moderne Opt, Inst Phys, Hausvogteipl 5-7, D-10117 Berlin, Germany. RI Vanne, Yulian/A-2361-2010; Jonsell, Svante/J-2251-2016 OI Vanne, Yulian/0000-0002-4623-2283; Jonsell, Svante/0000-0003-4969-1714 NR 14 TC 18 Z9 18 U1 0 U2 3 PU AMERICAN 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 JUN PY 2006 VL 73 IS 6 AR 062706 DI 10.1103/PhysRevA.73.062706 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 058WI UT WOS:000238694900085 ER PT J AU Kohri, K Moroi, T Yotsuyanagi, A AF Kohri, Kazunori Moroi, Takeo Yotsuyanagi, Akira TI Big-bang nucleosynthesis with unstable gravitino and upper bound on the reheating temperature SO PHYSICAL REVIEW D LA English DT Article ID PRIMORDIAL HELIUM ABUNDANCE; COSMOLOGICAL BARYON DENSITY; LATE-DECAYING PARTICLES; BLUE COMPACT GALAXIES; LIGHT-ELEMENTS; DEUTERIUM ABUNDANCE; EARLY UNIVERSE; HALO STARS; INFLATIONARY UNIVERSE; RELIC PARTICLES AB We study the effects of unstable gravitino on big-bang nucleosynthesis. If the gravitino mass is smaller than similar to 10 TeV, primordial gravitinos produced after inflation are likely to decay after big-bang nucleosynthesis starts, and light-element abundances may be significantly affected by hadro and photodissociation processes as well as by p <-> n conversion process. We calculate the light-element abundances and derive upper bounds on the reheating temperature after inflation. In our analysis, we calculate decay parameters of the gravitino (i.e. lifetime and branching ratios) in detail. In addition, we perform a systematic study of the hadron spectrum produced by the gravitino decay, taking account of all the hadrons produced by the decay products of the gravitino (including the daughter superparticles). We discuss model dependence of the upper bound on the reheating temperature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. Tohoku Univ, Dept Phys, Sendai, Miyagi 9808578, Japan. RP Kohri, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 85 TC 137 Z9 137 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN PY 2006 VL 73 IS 12 AR 123511 DI 10.1103/PhysRevD.73.123511 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 058XW UT WOS:000238698900020 ER PT J AU Herbst, W Dhital, S Francis, A Lin, LW Tresser, N Williams, E AF Herbst, W Dhital, S Francis, A Lin, LW Tresser, N Williams, E TI Evidence for differential rotation on a T Tauri star SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB Five years of photometric monitoring of the T Tauri star HBC 338 in NGC 1333 has revealed that it is a periodic variable, but the period has changed significantly with time. From 2000 to 2003, a period near 5.6 days was observed, while in the last two seasons, the dominant period is near 4.6 days. No other T Tauri star has been seen to change its period by such a large percentage. We propose a model in which a differentially rotating star is seen nearly equator-on and a high-latitude spot has gradually been replaced by a low-latitude spot. We show that this model provides an excellent fit to the observed shapes of the light curves at each epoch. The amplitude and sense of the inferred differential rotation are similar to what is seen on the Sun. This may be surprising, given the likely high degree of magnetic surface activity on the star relative to the Sun, but we note that HBC 338 is clearly an exceptional T Tauri star. C1 Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Herbst, W (reprint author), Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. EM wherbst@wesleyan.edu; sdhital1@swarthmore.edu; afrancis@hamilton.edu; ntresser@wesleyan.edu; ewilliams@wesleyan.edu NR 8 TC 8 Z9 8 U1 0 U2 0 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 JUN PY 2006 VL 118 IS 844 BP 828 EP 832 DI 10.1086/506481 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 057XS UT WOS:000238629100007 ER PT J AU Wolk, SJ Schulz, N Stauffer, J Evans, N Townsley, L Megeath, T Huenemoerder, D Leitherer, C Jayawardana, R AF Wolk, SJ Schulz, N Stauffer, J Evans, N Townsley, L Megeath, T Huenemoerder, D Leitherer, C Jayawardana, R TI Star Formation in the Era of the Three Great Observatories SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article; Proceedings Paper CT Workshop on Star Formation in the Era of Three Great Observatories CY JUL 13-15, 2005 CL Cambridge, MA SP Chandra X-Ray Ctr ID ORION NEBULA; CLUSTER C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 NR 11 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 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2006 VL 118 IS 844 BP 939 EP 946 DI 10.1086/505090 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 057XS UT WOS:000238629100020 ER PT J AU Landry, B Adamski, D Schmitz, P Parent, CE Roque-Albelo, L AF Landry, Bernard Adamski, David Schmitz, Patrick Parent, Christine E. Roque-Albelo, Lazaro TI Taygete sphecophila (Meyrick) (Lepidoptera; Autostichidae): redescription of the adult, description of the larva and pupa, and impact on Polistes wasps (Hymenoptera; Vespidae) nests in the Galapagos Islands SO REVUE SUISSE DE ZOOLOGIE LA English DT Article DE micro moths; autostichidae; Taygete; Polistes; Galapagos islands; mitochondrial DNA; larval predation; morphology; ecology ID SUBORDER DITRYSIA LEPIDOPTERA; LAST-STAGE LARVAE; MORPHOLOGICAL SURVEY; COLEOPHORIDAE; GELECHIOIDEA; MAXILLAE AB Taygete sphecophila (Meyrick) (Lepidoptera; Autostichidae) is reported on the Galapagos Islands. The morphology of the moth, larva, and pupa are described and illustrated in details. Part of the mitochondrial DNA was sequenced and made available on GenBank. The incidence of predation by T sphecophila on nests of Polistes versicolor Olivier (Hymenoptera; Vespidae) was measured in four different vegetation zones of Floreana and Santa Cruz Islands. The percentages of infested nests varied greatly (from 13.9% to 66.7% on Floreana and from 20.0 to 100% on Santa Cruz) and no clear ecological trends could be ascertained. C1 Nat Hist Museum, CH-1211 Geneva 6, Switzerland. Smithsonian Inst, Museum Natl Hist Nat, Dept Entomol, NHB,E523, Washington, DC 20013 USA. Nat Hist Museum, CH-1211 Geneva 6, Switzerland. Simon Fraser Univ, Dept Biol Sci, Behav Ecol Res Grp, Burnaby, BC V5A 1S6, Canada. Charles Darwin Res Stn, Dept Entomol, Quito, Ecuador. Univ Cardiff Wales, Cardiff Sch Biosci, Biodivers & Ecol Proc Res Grp, Cardiff CF10 3TL, Wales. RP Landry, B (reprint author), Nat Hist Museum, CP 6434, CH-1211 Geneva 6, Switzerland. EM bernard.landry@ville-ge.ch; dadamski@sel.barc.usda.gov; patrick.schmitz@ville-ge.ch; cparent@sfu.ca; lazaro@fcdarwin.ec.org NR 35 TC 7 Z9 8 U1 0 U2 5 PU MUSEUM HISTOIRE NATURELLE PI GENEVA 6 PA CASE POSTALE 6434, ATTN:DENISE MAIER ADMN REV SUISSE DE ZOOLOGIE, CH-L211 GENEVA 6, SWITZERLAND SN 0035-418X J9 REV SUISSE ZOOL JI Rev. Suisse Zool. PD JUN PY 2006 VL 113 IS 2 BP 307 EP 323 PG 17 WC Zoology SC Zoology GA 063OA UT WOS:000239027900010 ER PT J AU Smith, DA Ralls, K Cypher, BL Clark, HO Kelly, PA Williams, DF Maldonado, JE AF Smith, DA Ralls, K Cypher, BL Clark, HO Kelly, PA Williams, DF Maldonado, JE TI Relative abundance of endangered San Joaquin kit foxes (Vulpes macrotis mutica) based on scat-detection dog surveys SO SOUTHWESTERN NATURALIST LA English DT Article ID NONNATIVE RED FOXES; MOLECULAR TRACKING; SWIFT FOXES; COYOTES; FECES; DNA AB Although the San Joaquin kit fox (Vulpes macrotis mutica) has been a federally protected subspecies since 1967, current information on its status throughout much of its historical range is lacking. Since 1983, only 5 surveys have been conducted, and a recent recovery plan emphasized the need for better information on the status of this subspecies. Between 2001 and 2003, we attempted to obtain new information on this kit fox on specific public and private properties in 8 counties in the San Joaquin Valley, California, where knowledge of its current status was limited or poorly understood. We used a trained detection-dog to survey for kit fox, red fox (V vulpes), and gray fox (Urocyon cinereoargenteus) scats on selected properties, followed by species identification based on genetic analysis of DNA extracted from all scats collected. Despite extensive survey efforts (539 km), kit fox was only detected in Merced County, in the area of Santa Nella, where a small kit fox population was previously documented. Red fox scats were located in Alameda, San Joaquin, and Merced counties, and gray fox scats were located in Fresno County. Our results suggest that if kit foxes are present on the properties surveyed, they either occur at extremely low densities, rendering detection difficult, or only occur intermittently in these areas. In striking contrast, our previous surveys conducted with the same method in the southern part of the range found large numbers of kit fox scats in various areas, particularly in Kern and San Luis Obispo counties. We recommend that future conservation plans focus on preserving additional habitat in areas where kit foxes are relatively abundant, specifically western Kern County and the Ciervo-Panoche region. C1 Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. Conservat & Res Ctr, Smithsonians Natl Zool Pk, Washington, DC 20008 USA. Calif State Univ Stanislaus, ESRP, Fresno, CA 93727 USA. Smithsonian Inst, Natl Museum Nat Hist, Natl Zool Pk, Genet Program, Washington, DC 20008 USA. RP Smith, DA (reprint author), Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. EM debsmith@u.washington.edu RI Clark, Howard/A-7053-2009 OI Clark, Howard/0000-0001-8384-2163 NR 35 TC 11 Z9 12 U1 3 U2 28 PU SOUTHWESTERN ASSN NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 J9 SOUTHWEST NAT JI Southw. Natural. PD JUN PY 2006 VL 51 IS 2 BP 210 EP 219 DI 10.1894/0038-4909(2006)51[210:RAOESJ]2.0.CO;2 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 057KD UT WOS:000238593800010 ER PT J AU Golub, L AF Golub, L. TI Coronal dynamics and the AIA on SDO SO SPACE SCIENCE REVIEWS LA English DT Review DE solar corona; coronal activity; solar dynamics; SDO AB We provide a brief overview of present-day studies of inner corona dynamics, with examples of mass ejections (CME), flares and active region dynamics. While the names of the topics have not changed in several decades, the internal details and the language used to express the nature of the problem have changed considerably. We conclude with a short discussion of the contribution to studies of coronal dynamics to be expected from the Atmospheric Imager Assembly (AIA) on the Solar Dynamics Observatory. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Golub, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lgolub@cfa.harvard.edu NR 9 TC 6 Z9 6 U1 4 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JUN PY 2006 VL 124 IS 1-4 BP 23 EP 32 DI 10.1007/s11214-006-9097-7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 137VD UT WOS:000244319800003 ER PT J AU Jackson, JBC Erwin, DH AF Jackson, JBC Erwin, DH TI What can we learn about ecology and evolution from the fossil record? SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID COMMUNITY STRUCTURE; NORTH-AMERICA; COORDINATED STASIS; DEATH ASSEMBLAGES; MULTIPLE SCALES; POLLEN RECORD; PHASE-SHIFTS; CORAL-REEFS; ABUNDANCE; DYNAMICS AB The increased application of abundance data embedded within a more detailed and precise environmental context is enabling paleontologists to explore more rigorously the dynamics and underlying processes of ecological and evolutionary change in deep time. Several recent findings are of special theoretical interest. Community membership is commonly more stable and persistent than expected by chance, even in the face of the extreme environmental changes of the Ice Ages, and major evolutionary novelties commonly lie dormant for tens of millions of years before the ecological explosions of the clades that possess them. As we discuss here, questions such as these cannot be adequately addressed without the use of the fossil record. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. RP Jackson, JBC (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM jbjackson@ucsd.edu RI Erwin, Douglas/A-9668-2009 NR 79 TC 47 Z9 51 U1 3 U2 21 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUN PY 2006 VL 21 IS 6 BP 322 EP 328 DI 10.1016/j.tree.2006.03.017 PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 058XF UT WOS:000238697200007 PM 16769432 ER PT J AU Rappole, JH Compton, BW Leimgruber, P Robertson, J King, DI Renner, SC AF Rappole, JH Compton, BW Leimgruber, P Robertson, J King, DI Renner, SC TI Modeling movement of West Nile virus in the western hemisphere SO VECTOR-BORNE AND ZOONOTIC DISEASES LA English DT Article DE West Nile virus; migratory birdsm; modeling disease movement ID MIGRATORY BIRDS; MOSQUITOS; MEXICO AB We modeled West Nile virus (WNV) movement rates and patterns based on a migratory bird agent (the Swainson's Thrush) and a resident bird agent (the House Sparrow), and compared the results of these models with actual movement data to investigate the likelihood that the pattern of WNV outbreaks observed in the New World was consistent with migrant bird-mediated spread, as reported from the Old World. We found that, contrary to Old World patterns, WNV activity in the Western Hemisphere does not seem consistent with movement by infected migrant birds. Instead WNV spread appears best explained by a non-directional movement, perhaps that of dispersing resident birds. C1 Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Massachusetts, Holdsworth Nat Resources Ctr, Dept Nat Resources Conservat, Amherst, MA 01003 USA. Univ Massachusetts, Holdsworth Nat Resources Ctr, US Forest Serv, NE Expt Stn, Amherst, MA 01003 USA. RP Rappole, JH (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, 500 Remount Rd, Front Royal, VA 22630 USA. EM rappolej@si.edu RI Leimgruber, Peter/O-1304-2015; OI Leimgruber, Peter/0000-0002-3682-0153; Renner, Swen/0000-0002-6893-4219 NR 33 TC 27 Z9 31 U1 5 U2 7 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1530-3667 J9 VECTOR-BORNE ZOONOT JI Vector-Borne Zoonotic Dis. PD SUM PY 2006 VL 6 IS 2 BP 128 EP 139 DI 10.1089/vbz.2006.6.128 PG 12 WC Public, Environmental & Occupational Health; Infectious Diseases SC Public, Environmental & Occupational Health; Infectious Diseases GA 058PD UT WOS:000238676000003 PM 16796510 ER PT J AU Belanus, BJ AF Belanus, Betty J. TI American regional folklore: A sourcebook and research guide. SO WESTERN FOLKLORE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Belanus, BJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU CALIF FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SUM PY 2006 VL 65 IS 3 BP 361 EP 363 PG 3 WC Folklore SC Arts & Humanities - Other Topics GA 165EO UT WOS:000246287000018 ER PT J AU Bremner-Harrison, S Harrison, SWR Cypher, BL Murdoch, JD Maldonado, J Darden, SK AF Bremner-Harrison, S Harrison, SWR Cypher, BL Murdoch, JD Maldonado, J Darden, SK TI Development of a single-sampling noninvasive hair snare SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE DNA analysis; hair snare; noninvasive sampling; San Joaquin kit fox; swift fox; Vulpes macrotis mutica; V. velox ID FECAL DNA; FECES; MICROSATELLITES; REPEATS; SCAT; DOGS AB Noninvasive hair and fecal DNA sampling provides a means of collecting information on elusive species, while causing little or no disturbance. However, current methods of hair collection do not preclude multiple sampling, thus risking sample contamination. We developed a hair snare that prevents multiple sampling, is cost-effective, easy to construct, and safe for target and nontarget species. Our initial field tests on endangered San Joaquin kit foxes (Vulpes macrotis mutica) and swift foxes (Vulpes velox) suggest that this hair snare may be effective in collecting uncontaminated samples for DNA analysis. C1 Calif State Univ Stanislaus, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, Dept Conservat Biol, Washington, DC 20008 USA. Univ Copenhagen, Inst Biol, Dept Populat Biol, Anim Behav Grp, DK-2200 Copenhagen, Denmark. RP Bremner-Harrison, S (reprint author), Calif State Univ Stanislaus, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. EM sbremnerharrison@esrp.csustan.edu RI Darden, Safi/C-5940-2016; OI Darden, Safi/0000-0002-2567-7902; Bremner-Harrison, Samantha/0000-0003-4770-1376 NR 14 TC 14 Z9 14 U1 0 U2 18 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 USA SN 0091-7648 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD JUN PY 2006 VL 34 IS 2 BP 456 EP 461 DI 10.2193/0091-7648(2006)34[456:DOASNH]2.0.CO;2 PG 6 WC Biodiversity Conservation SC Biodiversity & Conservation GA 058ZB UT WOS:000238702000028 ER PT J AU Castillo, AMR Eberhard, JR AF Castillo, Angelica M. Rodriguez Eberhard, Jessica R. TI Reproductive behavior of the Yellow-crowned Parrot (Amazona ochrocephala) in western Panama SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID PUERTO-RICAN PARROTS; NESTING-BEHAVIOR; TREE HOLLOWS; AVAILABILITY; COCKATOOS; SURVIVAL; SITES AB We studied the breeding biology of the Panamanian subspecies of the Yellow-crowned Parrot, Amazona ochrocephala panantensis, during 1997-1999 in the province of Chiriqui, Panama, to provide basic information regarding the breeding behavior and reproductive success of these parrots in their natural habitat. We recorded parrot behaviors throughout the reproductive period, monitored nest success, and characterized occupied and non-occupied tree cavities. All breeding attempts involved a male-female pair. Clutch size ranged from 2 to 4 eggs, which were incubated only by the female, beginning when the first egg was laid. Incubation averaged 25 days and the eggs hatched asynchronously. During the incubation period, females remained inside the nest for long periods of time, though they often departed from the nest area during early mornings and late afternoons, presumably to forage; during this period, males were not observed entering the nest, though they often remained nearby. During the nestling period, males contributed significantly to feeding the offspring. Pairs nested in trees that were in good or fair condition, and did not favor cavities in any one tree species. As found in many other field studies of parrots, breeding success was low. Only 10% (1997-1998) and 14% (1998-1999) of the nests survived poaching and natural predation. Because nest poaching was the primary cause of breeding failure and poses a serious threat to population viability, we also present data on poaching techniques and the local trade of nestling parrots. Overall, the pool of breeding adults is likely made up of aging individuals that are not being replaced, setting the stage for a rapid population decline. Received 13 January 2005, accepted 23 November 2005. C1 Univ Chiriqui, Escuela Biol, David, Panama. Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, JR (reprint author), Louisiana State Univ, Dept Biol Sci, 202 Life Sci, Baton Rouge, LA 70803 USA. EM eberhard@lsu.edu NR 36 TC 15 Z9 17 U1 0 U2 1 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 JUN PY 2006 VL 118 IS 2 BP 225 EP 236 DI 10.1676/05-003.1 PG 12 WC Ornithology SC Zoology GA 055FV UT WOS:000238436300012 ER PT J AU Rey, AM Satija, II Clark, CW AF Rey, Ana Maria Satija, Indubala I. Clark, Charles W. TI Noise correlations of hard-core bosons: quantum coherence and symmetry breaking SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article; Proceedings Paper CT International Workshop on Theory of Quantum Gas and Quantum Coherence CY OCT 29-NOV 02, 2005 CL Cortona, ITALY ID TONKS-GIRARDEAU GAS; OPTICAL LATTICE; SYSTEMS; ATOMS AB Noise correlations, such as those observable in the time of flight images of a released cloud, are calculated for hard-core bosonic (HCBs) atoms. These second-order correlations are used to explore quantum coherence of strongly correlated bosons in the fermionized regime with and without external parabolic confinement. Our analysis points to distinctive new experimental signatures of the Mott phase. We also calculate noise correlations for the corresponding spin1/2 XY model onto which the HCB system is standardly mapped. Our study shows important differences between the two systems due to the contribution of multiply occupied virtual states in HCBs. Such states do not exist in spin models. An interesting manifestation of such states is the breaking of particle hole symmetry in HCB systems. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Ctr Astrophys, Cambridge, MA 02138 USA. NIST, Gaithersburg, MD 20899 USA. George Mason Univ, Dept Phys, Fairfax, VA 22030 USA. RP Rey, AM (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM arey@cfa.harvard.edu; isatija@physics.gmu.edu RI Clark, Charles/A-8594-2009 OI Clark, Charles/0000-0001-8724-9885 NR 25 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 28 PY 2006 VL 39 IS 10 SI SI BP S177 EP S190 DI 10.1088/0953-4075/39/10/S17 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 054LM UT WOS:000238378200018 ER PT J AU Vari, RP Ferraris, CJ AF Vari, RP Ferraris, CJ TI The catfish genus Tetranematichthys (Auchenipteridae) SO COPEIA LA English DT Article ID TASTE-BUDS; SILURIFORMES; BARBELS AB The neotropical auchenipterid catfish genus Tetranematichthys is reviewed. Tetranematichthys was previously thought to be monotypic with its single species, T. quadrifilis, reported to have a broad range encompassing major portions of the Amazon basin and southern tributaries of the Rio Orinoco. Tetranematichthys quadrifilis was rather found to be endemic to the Rio Guapore in the southwestern portions of the Amazon basin and a new species of the genus is described from material originating in the upper Rio Negro system in Brazil and Venezuela and the upper Rio Orinoco basin in southern Venezuela. The new species is also apparently widespread within the Amazon basin and the southern and north-central portions of the Rio Orinoco system. The species of Tetranematichthys have distinctive modifications of the mandibular barbel and associated systems, which are proposed as synapomorphic for the species of the genus and that potentially function as a fishing lure. RP Vari, RP (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Res Associate, POB 37012,WG-14,MRC-159, Washington, DC 20013 USA. EM varir@si.edu; carlferraris@comcast.net NR 45 TC 4 Z9 6 U1 0 U2 1 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 26 PY 2006 IS 2 BP 168 EP 180 DI 10.1643/0045-8511(2006)6[168:TCGTA]2.0.CO;2 PG 13 WC Zoology SC Zoology GA 049SF UT WOS:000238036200003 ER PT J AU Munroe, TA AF Munroe, TA TI New western Indian Ocean tonguefish (Pleuronectiformes : Cynoglossidae, Symphurus) SO COPEIA LA English DT Article ID PACIFIC AB Symphurus monostigmus, described on the basis of two males (48.8 and 54.6 mm SL) collected on the inner continental shelf at 65-110 m off the coast of KwaZulu-Natal, South Africa, is distinguished from congeners by the following combination of characters: an irregular, conspicuous dark spot overlying the anteroventral ocular-side body cavity; a 1-2-2-2-2 pattern of interdigitation of dorsal-fin pterygiophores and neural spines; 14 caudal-fin rays; 86 dorsal-fin rays; 73-74 anal-fin rays; 48 total vertebrae; five hypurals; black peritoneum (posterior region only); ocular side uniformly yellowish-white with numerous, darker reddish-brown freckles especially noticeable along dorsal and ventral contours of body (freckles coalesced into several darker blotches on dorsal and ventral margins on posterior half of body), blind side uniformly yellowish-white, and dorsal and anal fins without conspicuous spots or ocelli. Symphurus monostigmus is most similar to S. macrophthalmus, but differs from that species in ID pattern (1-2-2-1-2 in S. macraphthalmus) and its smaller eye (100-138 vs. 211 in thousandths of HL) with much smaller pupil (pupil diameter/eye diameter 28-32% vs. ca. 54% in S. macrophthalmus). C1 Smithsonian Inst, NOAA, Natl Marine Fisheries Serv, Natl Systemat Lab,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Munroe, TA (reprint author), Smithsonian Inst, NOAA, Natl Marine Fisheries Serv, Natl Systemat Lab,Natl Museum Nat Hist, Room WC57,MRC 0153, Washington, DC 20013 USA. EM munroet@si.edu NR 10 TC 8 Z9 8 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 26 PY 2006 IS 2 BP 230 EP 234 PG 5 WC Zoology SC Zoology GA 049SF UT WOS:000238036200010 ER PT J AU De Astarloa, JMD Munroe, TA Desoutter, M AF Diaz De Astarloa, Juan M. Munroe, Thomas A. Desoutter, Martine TI Redescription and holotype clarification of Paralichthys orbignyanus (Valenciennes, 1839) (Pleuronectiformes : Paralichthyidae) SO COPEIA LA English DT Article AB Collecting by Alcide D'Orbigny in the western South Atlantic provided material for Platessa orbignyana Valenciennes, 1839, published as an illustration of the holotype without accompanying descriptive information. A brief and inadequate description was provided in 1847. Thereafter, the holotype was thought to be lost, precluding comparative study and resulting in nomenclatural confusion for other nominal paraliclithyid species. A specimen of Paralichthys collected in the Rio de la Plata, Buenos Aires, Argentina by D'Orbigny at the Museum national d'histoire naturelle (MNHN 1999-0295) is here identified as the holotype of Platessa orbignyana Valenciennes, 1839. A redescription of the holotype and comparison with other South Atlantic species resolves several nomenclatural issues. C1 Univ Nacl Mar Del Plata, Fac Ciencias Exactas & Nat, Dept Ciencias Marinas, RA-7602 Mar Del Plata, Buenos Aires, Argentina. Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. Museum Natl Hist Nat, Dept Systemat & Evolut, Unite Taxon Collect, F-75231 Paris 05, France. RP De Astarloa, JMD (reprint author), Univ Nacl Mar Del Plata, Fac Ciencias Exactas & Nat, Dept Ciencias Marinas, Funes 3350, RA-7602 Mar Del Plata, Buenos Aires, Argentina. EM astarloa@mdp.edu.ar; munroet@si.edu; desoutte@mnhn.fr NR 47 TC 0 Z9 1 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD MAY 26 PY 2006 IS 2 BP 235 EP 243 PG 9 WC Zoology SC Zoology GA 049SF UT WOS:000238036200011 ER PT J AU Torres-Mendoza, D Gonzalez, J Ortega-Barria, E Heller, MV Capson, TL McPhail, K Gerwick, WH Cubilla-Rios, L AF Torres-Mendoza, Daniel Gonzalez, Jose Ortega-Barria, Eduardo Heller, Maria V. Capson, Todd L. McPhail, Kerry Gerwick, William H. Cubilla-Rios, Luis TI Weakly antimalarial flavonol arabinofuranosides from Calycolpus warszewiczianus SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID DRUG DISCOVERY; GLYCOSIDE; PARASITES; LEAVES AB Three new flavonol arabinosides (2-4) were isolated from the young leaves of Calycolpus warszewiczianus. The structures were determined as myricetin-3-O-alpha-L-3 ''-acetylarabinofuranoside (2), myricetin- 3-O-alpha-L-3 '',5 ''-diacetylarabinofuranoside (3), and 5-galloylquercetin-3-O-alpha-L-arabinofuranoside (4). Molecular structures were elucidated using NMR spectroscopy in combination with IR and MS data. Two known compounds, myricetin- 3-O-alpha-L-arabinofuranoside (1) and (-)-epicatechin (5), were also isolated. The compounds were tested in vitro against a chloroquine-resistant strain of Plasmodium falciparum, Leishmania mexicana, and Trypanosoma cruzi parasites. Compound 4 demonstrated weak activity against a chloroquine-resistant strain of P. falciparum (14.5 mu M), whereas none of the compounds demonstrated activity against L. mexicana and T. cruzi at the concentrations of 40 and 50 mu g/mL, respectively, and no cytotoxicity was detected against mammalian cells below 100 mu g/mL. C1 Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. Inst Invest Cientificas Avanzadas & Serv Alta Tec, Secretaria Nacl Ciencia Tecnol & Innov, Ancon, Panama. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Oregon State Univ, Corvallis, OR 97331 USA. RP Cubilla-Rios, L (reprint author), Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Apartado 0824-10835, Panama City, Panama. EM lucr@ancon.up.ac.pa OI Torres-Mendoza, Daniel/0000-0002-3540-4238 FU FIC NIH HHS [1U01 TW-006634-01] NR 23 TC 14 Z9 14 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD MAY 26 PY 2006 VL 69 IS 5 BP 826 EP 828 DI 10.1021/np050484i PG 3 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 046MW UT WOS:000237816700022 PM 16724851 ER PT J AU Mostepanenko, VM Babb, JF Caride, AO Klimchitskaya, GL Zanette, SI AF Mostepanenko, VM Babb, JF Caride, AO Klimchitskaya, GL Zanette, SI TI Dependence of the Casimir-Polder interaction between an atom and a cavity wall on atomic and material properties SO JOURNAL OF PHYSICS A-MATHEMATICAL AND GENERAL LA English DT Article; Proceedings Paper CT 7th Workshop on Quantum Field Theory under the Influence of External Conditions (QFEXT05) CY SEP 05-09, 2005 CL Barcelona, SPAIN ID SURFACES; TEMPERATURE AB The Casimir-Polder and van der Waals interactions between an atom and a flat cavity wall are investigated under the influence of real conditions including the dynamic polarizability of the atom, actual conductivity of the wall material and nonzero temperature of the wall. The cases of different atoms near metal and dielectric walls are considered. It is shown that to obtain accurate results for the atom-wall interaction at short separations, one should use the complete tabulated optical data for the complex refractive index of the wall material and the accurate dynamic polarizability of an atom. At relatively large separations in the case of a metal wall, one may use the plasma model dielectric function to describe the dielectric properties of the wall material. The obtained results are important for the theoretical interpretation of experiments on quantum reflection and Bose-Einstein condensation. C1 Noncommercial Partnership Sci Instruments, Moscow, Russia. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil. NW Tech Univ, St Petersburg, Russia. RP Mostepanenko, VM (reprint author), Noncommercial Partnership Sci Instruments, Moscow, Russia. OI Babb, James/0000-0002-3883-9501 NR 22 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0305-4470 J9 J PHYS A-MATH GEN JI J. Phys. A-Math. Gen. PD MAY 26 PY 2006 VL 39 IS 21 BP 6583 EP 6587 DI 10.1088/0305-4470/39/21/S57 PG 5 WC Physics, Multidisciplinary; Physics, Mathematical SC Physics GA 054NM UT WOS:000238384200058 ER PT J AU Pogue, MG AF Pogue, Michael G. TI The Noctuinae (Lepidoptera : Noctuidae) of Great Smoky Mountains National Park, USA SO ZOOTAXA LA English DT Article DE systematics; All Taxa Biodiversity Inventory; North Carolina; Tennessee; moths AB Forty-eight species of Noctuinae are recorded from Great Smoky Mountains National Park, Tennessee and North Carolina, U. S. A., with 17 species in the tribe Agrotini and 31 species in the tribe Noctuini. Images of adults, description/diagnosis, flight period, collected localities, abundance, elevational range, general distribution, and larval hosts are presented for each species. The greatest diversity of Noctuinae species ( n= 29) was recorded from four combined localities along Big Cove Road, Swain Co., North Carolina. C1 Smithsonian Inst, Systemat Entomol Lab, PSI, ARS,USDA, Washington, DC 20013 USA. RP Pogue, MG (reprint author), Smithsonian Inst, Systemat Entomol Lab, PSI, ARS,USDA, POB 37012,NMNH,MRC-168, Washington, DC 20013 USA. EM mpogue@sel.barc.usda.gov NR 23 TC 6 Z9 7 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 MAY 26 PY 2006 IS 1215 BP 1 EP 90 PG 90 WC Zoology SC Zoology GA 046KB UT WOS:000237809400001 ER PT J AU Butt, YM Drake, J Benaglia, P Combi, JA Dame, T Miniati, F Romero, GE AF Butt, YM Drake, J Benaglia, P Combi, JA Dame, T Miniati, F Romero, GE TI Deeper Chandra follow-up of Cygnus TeV source perpetuates mystery SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays : observations; ISM : bubbles; open clusters and associations : individual (Cygnus OB2) ID RAY SOURCE; OB2; ASSOCIATIONS; CLUSTER; NEBULA AB A 50 ks Chandra observation of the unidentified TeV source in Cygnus reported by the HEGRA collaboration reveals no obvious diffuse X-ray counterpart. However, 240 pointlike X-ray sources are detected within or nearby the extended TeV J2032+4130 source region, of which at least 36 are massive stars and two may be radio emitters. That the HEGRA source is a composite, having as a counterpart the multiple pointlike X-ray sources we observe, cannot be ruled out. Indeed, the distribution of pointlike X-ray sources appears nonuniform and concentrated broadly within the extent of the TeV source region. We offer a hypothesis for the origin of the very high energy gamma-ray emission in Cyg OB2 based on the local acceleration of TeV-range cosmic rays and the differential distribution of OB versus less massive stars in this association. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Argentino Radioastron, RA-1894 Buenos Aires, DF, Argentina. Natl Univ La Plata, Fac Ciencias Astron & Geofis, RA-1900 La Plata, Argentina. Univ Jaen, Dept Fis, Jaen 23071, Spain. ETH, Dept Phys, CH-8093 Zurich, Switzerland. RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 24 TC 26 Z9 26 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2006 VL 643 IS 1 BP 238 EP 244 DI 10.1086/502642 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043TP UT WOS:000237624900024 ER PT J AU Faucher-Giguere, CA Kaspi, VM AF Faucher-Giguere, Claude-Andre Kaspi, Victoria M. TI Birth and evolution of isolated radio pulsars SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxy : structure; methods : statistical; pulsars : general; stars : kinematics; stars : neutron ID PROPER-MOTION MEASUREMENTS; HIGH-FREQUENCY SURVEY; DATA-ANALYSIS SYSTEMS; INITIAL SPIN PERIOD; YOUNG NEUTRON-STARS; GAMMA-RAY PULSARS; GALACTIC DISTRIBUTION; VELOCITY DISTRIBUTION; PSR B1913+16; POPULATION SYNTHESIS AB We investigate the birth and evolution of Galactic isolated radio pulsars. We begin by estimating their birth space velocity distribution from proper-motion measurements of Brisken and coworkers. We find no evidence for multimodality of the distribution and favor one in which the absolute one-dimensional velocity components are exponentially distributed and with a three-dimensional mean velocity of 380(-60)(+40) km s(-1). We then proceed with a Monte Carlo based population synthesis, modeling the birth properties of the pulsars, their time evolution, and their detection in the Parkes and Swinburne Multibeam surveys. We present a population model that appears generally consistent with the observations. Our results suggest that pulsars are born in the spiral arms, with a galactocentric radial distribution that is well described by the functional form proposed by Yusifov & Kucuk, in which the pulsar surface density peaks at radius similar to 3 kpc. The birth spin period distribution extends to several hundred milliseconds, with no evidence of multimodality. Models that assume the radio luminosities of pulsars to be independent of the spin periods and period derivatives are inadequate, as they lead to the detection of too many old simulated pulsars in our simulations. Dithered radio luminosities proportional to the square root of the spin-down luminosity accommodate the observations well and provide a natural mechanism for the pulsars to dim uniformly as they approach the death line, avoiding an observed pileup on the latter. There is no evidence for significant torque decay ( due to magnetic field decay or otherwise) over the lifetime of the pulsars as radio sources ( similar to 100 Myr). Finally, we estimate the pulsar birthrate and total number of pulsars in the Galaxy. C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RP Faucher-Giguere, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cgiguere@cfa.harvard.edu NR 151 TC 293 Z9 295 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 MAY 20 PY 2006 VL 643 IS 1 BP 332 EP 355 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043TP UT WOS:000237624900033 ER PT J AU Williams, BF Naik, S Garcia, MR Callanan, PJ AF Williams, BF Naik, S Garcia, MR Callanan, PJ TI A catalog of transient X-ray sources in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; galaxies : individual (M31); X-rays : binaries; X-rays : stars ID XMM-NEWTON OBSERVATIONS; PLANE CHAMPLANE SURVEY; AQUILA X-1; CENTRAL REGION; LIGHT CURVES; BLACK-HOLES; CHANDRA; BINARIES; DISCOVERY; POLARS AB From 1999 October to 2002 August, 45 transient X-ray sources were detected in M31 by Chandra and XMM-Newton. We have performed spectral analysis of all XMM-Newton and Chandra ACIS detections of these sources, as well as flux measurements of Chandra HRC detections. The result is absorption-corrected X-ray light curves for these sources covering this 2.8 yr period, along with spectral parameters for several epochs of the outbursts of most of the transient sources. We supply a catalog of the locations, outburst dates, peak observed luminosities, decay time estimates, and spectral properties of the transient sources, and we discuss similarities with Galactic X-ray novae. Duty cycle estimates are possible for eight of the transients and range from 34% to 2%; upper limits to the duty cycles are estimated for an additional 15 transients and cover a similar range. We find five transients that have rapid decay times and may be ultracompact X-ray binaries. Spectra of three of the transients suggest that they may be faint Galactic foreground sources. If even one is a foreground source, this suggests a surface density of faint transient X-ray sources of >= 1 deg(-2). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head-cfa.harvard.edu; sachi@ucc.ie; garcia@head-cfa.harvard.edu; paulc@ucc.ie NR 57 TC 26 Z9 26 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2006 VL 643 IS 1 BP 356 EP 375 DI 10.1086/501496 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043TP UT WOS:000237624900034 ER PT J AU Albert, J Aliu, E Anderhub, H Antoranz, P Armada, A Asensio, M Baixeras, C Barrio, JA Bartelt, M Bartko, H Bastieri, D Bavikadi, SR Bednarek, W Berger, K Bigongiari, C Biland, A Bisesi, E Bock, RK Bordas, P Bosch-Ramon, V Bretz, T Britvitch, I Camara, M Carmona, E Chilingarian, A Ciprini, S Coarasa, JA Commichau, S Contreras, JL Cortina, J Curtef, V Dame, TM Danielyan, V Dazzi, F De Angelis, A Reyes, RDL De Lotto, B Domingo-Santamari, E Dorner, D Doro, M Errando, M Fagiolini, M Ferenc, D Fernandez, E Firpo, R Flix, J Fonseca, MV Font, L Fuchs, M Galante, N Garczarczyk, M Gaug, M Giller, M Goebel, F Hakobyan, D Hayashida, M Hengstebeck, T Hohne, D Hose, J Hsu, CC Isar, PG Jacon, P Kalekin, O Kasyra, R Kranich, D Laatiaoui, M Laille, A Lenisa, T Liebing, P Lindfors, E Lombardi, S Longo, F Lopez, J Lopez, M Lorenz, E Lucarelli, F Majumdar, P Maneva, G Mannheim, K Mansutti, O Mariotti, M Martinez, M Mase, K Mazin, D Merck, C Meucci, M Meyer, M Miranda, JM Mirzoyan, R Mizobuchi, S Moralejo, A Nilsson, K Ona-Wilhelmi, E Orduna, R Otte, N Oya, I Paneque, D Paoletti, R Paredes, JM Pasanen, M Pascoli, D Pauss, F Pavel, N Pegna, R Persic, M Peruzzo, L Piccioli, A Poller, M Prandini, E Raymers, A Rico, J Rhode, W Ribo, M Riegel, B Rissi, M Robert, A Rugamer, S Saggion, A Sanchez, A Sartori, P Scalzotto, V Scapin, V Schmitt, R Schweizer, T Shayduk, M Shinozaki, K Shore, SN Sidro, N Sillanpaa, A Sobczynska, D Stamerra, A Stark, LS Takalo, L Temnikov, P Tescaro, D Teshima, M Tonello, N Torres, A Torres, DF Turini, N Vankov, H Vitale, V Wagner, RM Wibig, T Wittek, W Zanin, R Zapatero, J AF Albert, J Aliu, E Anderhub, H Antoranz, P Armada, A Asensio, M Baixeras, C Barrio, JA Bartelt, M Bartko, H Bastieri, D Bavikadi, SR Bednarek, W Berger, K Bigongiari, C Biland, A Bisesi, E Bock, RK Bordas, P Bosch-Ramon, V Bretz, T Britvitch, I Camara, M Carmona, E Chilingarian, A Ciprini, S Coarasa, JA Commichau, S Contreras, JL Cortina, J Curtef, V Dame, TM Danielyan, V Dazzi, F De Angelis, A Reyes, RDL De Lotto, B Domingo-Santamari, E Dorner, D Doro, M Errando, M Fagiolini, M Ferenc, D Fernandez, E Firpo, R Flix, J Fonseca, MV Font, L Fuchs, M Galante, N Garczarczyk, M Gaug, M Giller, M Goebel, F Hakobyan, D Hayashida, M Hengstebeck, T Hohne, D Hose, J Hsu, CC Isar, PG Jacon, P Kalekin, O Kasyra, R Kranich, D Laatiaoui, M Laille, A Lenisa, T Liebing, P Lindfors, E Lombardi, S Longo, F Lopez, J Lopez, M Lorenz, E Lucarelli, F Majumdar, P Maneva, G Mannheim, K Mansutti, O Mariotti, M Martinez, M Mase, K Mazin, D Merck, C Meucci, M Meyer, M Miranda, JM Mirzoyan, R Mizobuchi, S Moralejo, A Nilsson, K Ona-Wilhelmi, E Orduna, R Otte, N Oya, I Paneque, D Paoletti, R Paredes, JM Pasanen, M Pascoli, D Pauss, F Pavel, N Pegna, R Persic, M Peruzzo, L Piccioli, A Poller, M Prandini, E Raymers, A Rico, J Rhode, W Ribo, M Riegel, B Rissi, M Robert, A Rugamer, S Saggion, A Sanchez, A Sartori, P Scalzotto, V Scapin, V Schmitt, R Schweizer, T Shayduk, M Shinozaki, K Shore, SN Sidro, N Sillanpaa, A Sobczynska, D Stamerra, A Stark, LS Takalo, L Temnikov, P Tescaro, D Teshima, M Tonello, N Torres, A Torres, DF Turini, N Vankov, H Vitale, V Wagner, RM Wibig, T Wittek, W Zanin, R Zapatero, J TI Observation of VHE gamma radiation from HESS J1834-087/W41 with the MAGIC telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations; supernova remnants ID SUPERNOVA-REMNANTS; RAY SOURCES; MILKY-WAY; EMISSION AB Recently, the HESS array has reported the detection of gamma-ray emission above a few hundred GeV from eight new sources located close to the Galactic plane. The source HESS J1834 - 087 is spatially coincident with the supernova remnant G23.3 - 0.3 (W41). Here we present MAGIC observations of this source, resulting in the detection of a differential gamma-ray flux consistent with a power law, described as dN(gamma)/(dA dt dE) = (3.7 +/- 0.6) x 10(-12) (E/TeV)(-2.5 +/- 0.2) cm(-2) s(-1) TeV-1. We confirm the extended character of this flux. We briefly discuss the observational technique used and the procedure implemented for the data analysis, and we put this detection in the perspective of the molecular environment found in the region of W41. We present (CO)-C-13 and (CO)-C-12 emission maps showing the existence of a massive molecular cloud in spatial superposition with the MAGIC detection. C1 Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. Inst Fis Altes Energies, E-08193 Barcelona, Spain. ETH, CH-8093 Zurich, Switzerland. Univ Complutense, E-28040 Madrid, Spain. Univ Autonoma Barcelona, E-08193 Bellaterra, Spain. Univ Dortmund, D-44227 Dortmund, Germany. Univ Wurzburg, D-97074 Wurzburg, Germany. Univ Padua, I-35131 Padua, Italy. Ist Nazl Fis Nucl, I-35131 Padua, Italy. Univ Udine, I-33100 Udine, Italy. INFN Trieste, I-33100 Udine, Italy. Univ Lodz, PL-90236 Lodz, Poland. Univ Barcelona, E-08028 Barcelona, Spain. Yerevan Phys Inst, AM-375036 Yerevan, Armenia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Siena, I-53100 Siena, Italy. INFN Pisa, I-53100 Siena, Italy. Univ Calif Davis, Davis, CA 95616 USA. Humboldt Univ, D-12489 Berlin, Germany. Tuorla Observ, FI-21500 Piikkio, Finland. Univ Trieste, I-34100 Trieste, Italy. Ist Nazl Fis Nucl, I-34100 Trieste, Italy. Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria. Osserv Astron Trieste, I-34100 Trieste, Italy. Univ Pisa, I-56126 Pisa, Italy. INFN Pisa, I-56126 Pisa, Italy. Inst Ciencies Espai, E-08193 Barcelona, Spain. RP Albert, J (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. RI Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Antoranz, Pedro/H-5095-2015; Fonseca Gonzalez, Maria Victoria/I-2004-2015; Miranda, Jose Miguel/F-2913-2013; Flix, Josep/G-5414-2012; Maneva, Galina/L-7120-2016; Torres, Diego/O-9422-2016; Temnikov, Petar/L-6999-2016; Laatiaoui, Mustapha/Q-6295-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; De Angelis, Alessandro/B-5372-2009; Isar, Paula Gina/B-5808-2011; Mannheim, Karl/F-6705-2012; Doro, Michele/F-9458-2012; chilingarian, ashot/B-1901-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Rico, Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Lopez Moya, Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014; Fernandez, Enrique/L-5387-2014; Tonello, Nadia/L-8065-2014; OI Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Antoranz, Pedro/0000-0002-3015-3601; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Miranda, Jose Miguel/0000-0002-1472-9690; Flix, Josep/0000-0003-2688-8047; Torres, Diego/0000-0002-1522-9065; Temnikov, Petar/0000-0002-9559-3384; Laatiaoui, Mustapha/0000-0003-0105-8303; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Doro, Michele/0000-0001-9104-3214; chilingarian, ashot/0000-0002-2018-9715; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Rico, Javier/0000-0003-4137-1134; Lopez Moya, Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Fernandez, Enrique/0000-0002-6405-9488; Tonello, Nadia/0000-0003-0550-1667; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Bordas, Pol/0000-0002-0266-8536; Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Lucarelli, Fabrizio/0000-0002-6311-764X; Persic, Massimo/0000-0003-1853-4900; Mansutti, Oriana/0000-0001-5758-4658; Hsu, Ching-Cheng/0000-0001-9406-2023; De Angelis, Alessandro/0000-0002-3288-2517; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Bigongiari, Ciro/0000-0003-3293-8522; De Lotto, Barbara/0000-0003-3624-4480; Bastieri, Denis/0000-0002-6954-8862 NR 31 TC 43 Z9 44 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2006 VL 643 IS 1 BP L53 EP L56 DI 10.1086/504917 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043TQ UT WOS:000237625000014 ER PT J AU Hoogerwerf, R Brickhouse, NS Mauche, CW AF Hoogerwerf, R Brickhouse, NS Mauche, CW TI Accretion column structure of magnetic cataclysmic variables from X-ray spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars : individual (EX Hydrae); techniques : spectroscopic; X-rays : stars ID EX-HYDRAE; WHITE-DWARF; LIGHT CURVES; EMISSION; REGION; IMAGES; FLOWS; DISKS; MASS; HYA AB Using Chandra HETG data, we present light curves for individual spectral lines of Mg XI and Mg XII for EX Hydrae, an intermediate polar - type cataclysmic variable. The Mg xi light curve, folded on the white dwarf spin period, shows two spikes that are not seen in the Mg XII or broadband light curves. Occultation of the accretion column by the body of the white dwarf would produce such spikes for an angle between the rotation axis and the accretion columns of alpha = 18 degrees and a height of the Mg xi emission above the white dwarf surface of less than or similar to 0.0004 white dwarf radii, or less than or similar to 4 km. The absence of spikes in the Mg XII and broadband light curves could then be explained if the bulk of its emission forms at much larger height, more than 0.004 white dwarf radii or over 40 km, above the white dwarf surface, although this is not consistent with the predictions of the standard Aizu model of the accretion column. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Hoogerwerf, R (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Mail Stop 31,60 Garden St, Cambridge, MA 02138 USA. EM rhoogerwerf@cfa.harvard.edu; nbrickhouse@cfa.harvard.edu; mauche@cygnus.llnl.gov OI Brickhouse, Nancy/0000-0002-8704-4473 NR 22 TC 5 Z9 5 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2006 VL 643 IS 1 BP L45 EP L48 DI 10.1086/505029 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 043TQ UT WOS:000237625000012 ER PT J AU Williams, RME Zimbelman, JR Johnston, AK AF Williams, RME Zimbelman, JR Johnston, AK TI Aspects of alluvial fan shape indicative of formation process: A case study in southwestern California with application to Mojave Crater fans on Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LASER ALTIMETER AB Longitudinal profiles from six alluvial fans surveyed in southwestern California have quantitative attributes that can distinguish formation processes. The radial slope of fans where debris flow processes dominated is constant while fluvially-fed fans have a concave-upward shape. We find the power law regression of upstream slope-distance profiles is the preferred approach for assessing concavity. Concavity index, the exponential determined via power law regression analysis, is an accurate reflection of the magnitude of the concavity and thus a qualitative measure of the relative influence of fluvial processes on the fan. Fan length and surface gradient are inversely correlated: debris flow fans are shorter and steeper (> 15 degrees) than their fluvial counterparts. The results of this investigation provide criteria to evaluate hypothesized formation processes and provide constraints on the amount of fluid and timescales involved in the generation of comparably-sized fans within Mojave Crater, Mars. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Williams, RME (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20013 USA. EM williams@psi.edu NR 13 TC 11 Z9 11 U1 0 U2 2 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 MAY 19 PY 2006 VL 33 IS 10 AR L10201 DI 10.1029/2005GL025618 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 049EJ UT WOS:000237998400001 ER PT J AU Barnett, R Petrov, D Lukin, M Demler, E AF Barnett, R Petrov, D Lukin, M Demler, E TI Quantum magnetism with multicomponent dipolar molecules in an optical lattice SO PHYSICAL REVIEW LETTERS LA English DT Article AB We consider bosonic dipolar molecules in an optical lattice prepared in a mixture of different rotational states. The 1/r(3) interaction between molecules for this system is produced by exchanging a quantum of angular momentum between two molecules. We show that the Mott states of such systems have a large variety of quantum phases characterized by dipolar orderings including a state with an ordering wave vector that can be changed by tilting the lattice. As the Mott insulating phase is melted, we also describe several exotic superfluid phases that will occur. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Barnett, R (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. OI Barnett, Ryan/0000-0002-5122-2856 NR 23 TC 99 Z9 100 U1 0 U2 5 PU AMERICAN 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 MAY 19 PY 2006 VL 96 IS 19 AR 190401 DI 10.1103/PhysRevLett.96.190401 PG 4 WC Physics, Multidisciplinary SC Physics GA 044PB UT WOS:000237683600002 PM 16803088 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, JSB Loeb, A TI Suppression of dwarf galaxy formation by cosmic reionization SO NATURE LA English DT Article ID STAR-FORMATION RATE; LY-ALPHA EMITTERS; LOW-MASS GALAXIES; HIGH-REDSHIFT; UNIVERSE; PHOTOIONIZATION; FEEDBACK AB A large number of faint galaxies, born less than a billion years after the Big Bang, have recently been discovered(1-6). Fluctuations in the distribution of these galaxies contributed to a scatter in the ionization fraction of cosmic hydrogen on scales of tens of megaparsecs, as observed along the lines of sight to the earliest known quasars(7-9). Theoretical simulations predict that the formation of dwarf galaxies should have been suppressed after cosmic hydrogen was reionized(10-13), leading to a drop in the cosmic star-formation rate(14). Here we report evidence for this suppression. We show that the post-reionization galaxies that produced most of the ionizing radiation at a redshift z approximate to 5.5 must have had a mass in excess of similar to 10(10.9+/-0.5) solar masses (M-.) or else the aforementioned scatter would have been smaller than observed. This limiting mass is two orders of magnitude larger than the galaxy mass that is thought to have dominated the reionization of cosmic hydrogen (similar to 10(8) M-.). We predict that future surveys with space-based infrared telescopes will detect a population of smaller galaxies that reionized the Universe at an earlier time, before the epoch of dwarf galaxy suppression. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Melbourne, Parkville, Vic 3010, Australia. RP Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swyithe@physics.unimelb.edu.au; aloeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 NR 33 TC 30 Z9 30 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 MAY 18 PY 2006 VL 441 IS 7091 BP 322 EP 324 DI 10.1038/nature04748 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 043IB UT WOS:000237593200041 PM 16710415 ER PT J AU Turner, BL Newman, S Reddy, KR AF Turner, BL Newman, S Reddy, KR TI Overestimation of organic phosphorus in wetland soils by alkaline extraction and molybdate colorimetry SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID NUCLEAR-MAGNETIC-RESONANCE; HUMIC-ACID; SEQUENTIAL EXTRACTION; NORTHERN EVERGLADES; FORMS; FRACTIONS; RETENTION; PHOSPHATE; P-31-NMR; PEAT AB Accurate information on the chemical nature of soil phosphorus is essential for understanding its bioavailability and fate in wetland ecosystems. Solution phosphorus-31 nuclear magnetic resonance (P-31 NMR) spectroscopy was used to assess the conventional colorimetric procedure for phosphorus speciation in alkaline extracts of organic soils from the Florida Everglades. Molybdate colorimetry markedly overestimated organic phosphorus by between 30 and 54% compared to NMR spectroscopy. This was due in large part to the association of inorganic phosphate with organic matter, although the error was exacerbated in some samples by the presence of pyrophosphate, an inorganic polyphosphate that is not detected by colorimetry. The results have important implications for our understanding of phosphorus biogeochemistry in wetlands and suggest that alkaline extraction and solution P-31 NMR spectroscopy is the only accurate method for quantifying organic phosphorus in wetland soils. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. S Florida Water Management Dist, Everglades Div, W Palm Beach, FL 33406 USA. Univ Florida, Dept Soil & Water Sci, Wetland Biogeochem Lab, Gainesville, FL 32611 USA. 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 44 TC 36 Z9 38 U1 2 U2 35 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAY 15 PY 2006 VL 40 IS 10 BP 3349 EP 3354 DI 10.1021/es052442m PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 042JZ UT WOS:000237525500038 PM 16749704 ER PT J AU Fergus, R Fry, M Karesh, WB Marra, PP Newman, S Paul, E AF Fergus, R Fry, M Karesh, WB Marra, PP Newman, S Paul, E TI Migratory birds and avian flu SO SCIENCE LA English DT Letter C1 Natl Audubon Soc, Ivyland, PA 18974 USA. Amer Bird Conservancy, Pesticides & Birds Program, Washington, DC 20009 USA. Wildlife Conservat Soc, Field Vet Program, Bronx, NY 10460 USA. Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Ornithol Council, Washington, DC 20006 USA. Wildlife Trust, New York, NY 10001 USA. RP Fergus, R (reprint author), Natl Audubon Soc, 545 Almshouse Rd, Ivyland, PA 18974 USA. NR 1 TC 14 Z9 15 U1 0 U2 10 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 MAY 12 PY 2006 VL 312 IS 5775 BP 845 EP 846 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 041JQ UT WOS:000237452900015 PM 16690841 ER PT J AU Polletta, MDC Wilkes, BJ Siana, B Lonsdale, CJ Kilgard, R Smith, HE Kim, DW Owen, F Efstathiou, A Jarrett, T Stacey, G Franceschini, A Rowan-Robinson, M Babbedge, TSR Berta, S Fang, F Farrah, D Gonzalez-Solares, E Morrison, G Surace, JA Shupe, DL AF del Carmen Polletta, Maria Wilkes, Belinda J. Siana, Brian Lonsdale, Carol J. Kilgard, Roy Smith, Harding E. Kim, Dong-Woo Owen, Frazer Efstathiou, Andreas Jarrett, Tom Stacey, Gordon Franceschini, Alberto Rowan-Robinson, Michael Babbedge, Tom S. R. Berta, Stefano Fang, Fan Farrah, Duncan Gonzalez-Solares, Eduardo Morrison, Glenn Surace, Jason A. Shupe, Dave L. TI Chandra and Spitzer unveil heavily obscured quasars in the Chandra/SWIRE survey SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : active; infrared : galaxies; quasars : individual (SWIRE J104409.95+585224.8; SWIRE J104406.30+583954.1); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED GALAXIES; SMALL MAGELLANIC CLOUD; X-RAY-ABSORPTION; DEEP FIELD-SOUTH; XMM-NEWTON; BLACK-HOLES; SPACE-TELESCOPE AB Using the large multiwavelength data set in the Chandra/SWIRE Survey (0.6 deg(2) in the Lockman Hole), we show evidence for the existence of highly obscured (Compton-thick) AGNs, estimate a lower limit to their surface density, and characterize their multiwavelength properties. Two independent selection methods based on the X-ray and infrared spectral properties are presented. The two selected samples contain ( 1) five X-ray sources with hard X-ray spectra and column densities greater than or similar to 10(24) cm(-2) and ( 2) 120 infrared sources with red and AGN-dominated infrared SEDs. We estimate a surface density of at least 25 Compton-thick AGNs deg(-2) detected in the infrared in the Chandra/SWIRE field, of which similar to 40% show distinct AGN signatures in their optical/near-infrared SEDs, the remaining being dominated by the host galaxy emission. Only similar to 33% of all Compton-thick AGNs are detected in the X-rays at our depth [F( 0: 3 8 keV) > 10(-15) ergs cm-(2) s(-1)]. We report the discovery of two sources in our sample of Compton-thick AGNs, SWIRE J104409.95+585224.8 (z = 2.54) and SWIRE J104406.30+583954.1 (z = 2.43), which are the most luminous Compton-thick AGNs at high z currently known. The properties of these two sources are discussed in detail with an analysis of their spectra, SEDs, luminosities, and black hole masses. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Cyprus Coll, Sch Comp Sci & Engn, CY-1516 Nicosia, Cyprus. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. Univ London Imperial Coll Sci & Technol, Blackett Lab, Astrophys Grp, London SW7 2BW, England. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Canada France Hawaii Telescope, Kamuela, HI 96743 USA. RP Polletta, MDC (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 124 TC 172 Z9 172 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 MAY 10 PY 2006 VL 642 IS 2 BP 673 EP 693 DI 10.1086/500821 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200005 ER PT J AU Dong, SB DePoy, DL Gaudi, BS Gould, A Han, C Park, BG Pogge, RW Udalski, A Szewczyk, O Kubiak, M Szymanski, MK Pietrzynski, G Soszynski, I Wyrzykowski, X Zebrun, K AF Dong, Subo DePoy, D. L. Gaudi, B. S. Gould, A. Han, C. Park, B. -G. Pogge, R. W. Udalski, A. Szewczyk, O. Kubiak, M. Szymanski, M. K. Pietrzynski, G. Soszynski, I. Wyrzykowski, X. Zebrun, K. TI Planetary detection efficiency of the magnification 3000 microlensing event OGLE-2004-BLG-343 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : bulge; gravitational lensing; planetary systems; stars : low-mass; brown dwarfs ID GALACTIC BULGE; EXTRASOLAR PLANETS; GRAVITATIONAL LENS; MASS; COMPANIONS; STELLAR; SYSTEMS; STAR; CONSTRAINTS; EXTINCTION AB OGLE-2004-BLG-343 was a microlensing event with peak magnification A(max) = 3000 +/- 1100, by far the highest magnification event ever analyzed and hence potentially extremely sensitive to planets orbiting the lens star. Due to human error, intensive monitoring did not begin until 43 minutes after peak, at which point the magnification had fallen to A similar to 1200, still by far the highest ever observed. As the light curve does not show significant deviations due to a planet, we place upper limits on the presence of such planets by extending the method of Yoo et al. (2004b), which combines light-curve analysis with priors from a Galactic model of the source and lens populations, to take account of finite-source effects. This is the first event so analyzed for which finite-source effects are important, and hence we develop two new techniques for evaluating these effects. Somewhat surprisingly, we find that OGLE-2004-BLG-343 is no more sensitive to planets than two previously analyzed events with A(max) similar to 100, despite the fact that it was observed at similar to 12 times higher magnification. However, we show that had the event been observed over its peak, it would have been sensitive to almost all Neptune-mass planets over a factor of 5 of projected separation and even would have had some sensitivity to Earth-mass planets. This shows that some microlensing events being detected in current experiments are sensitive to very low mass planets. We also give suggestions on how extremely high magnification events can be more promptly monitored in the future. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea. Korea Astron & space Sci Inst, Taejon 305348, South Korea. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Concepcion, Concepcion, Chile. RP Dong, SB (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM dong@astronomy.ohio-state.edu; depoy@astronomy.ohio-state.edu; sgaudi@cfa.harvard.edu; gould@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; bgpark@kasi.re.kr; pogge@astronomy.ohio-state.edu; udalski@astrouw.edu.pl; szewczyk@astrouw.edu.pl; mk@astrouw.edu.pl; msz@astrouw.edu.pl; pietrzyn@astrouw.edu.pl; soszynsk@astrouw.edu.pl; wyrzykow@astrouw.edu.pl; zebrun@astrouw.edu.pl RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012 NR 52 TC 81 Z9 81 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 MAY 10 PY 2006 VL 642 IS 2 BP 842 EP 860 DI 10.1086/501224 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200019 ER PT J AU Young, ET Teixeira, PS Lada, CJ Muzerolle, J Persson, SE Murphy, DC Siegler, N Marengo, M Krause, O Mainzer, AK AF Young, ET Teixeira, PS Lada, CJ Muzerolle, J Persson, SE Murphy, DC Siegler, N Marengo, M Krause, O Mainzer, AK TI Spitzer and Magellan observations of NGC 2264: A remarkable star-forming core near IRS 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2264); stars : formation; stars : pre-main-sequence ID INITIAL MASS FUNCTION; MULTIBAND IMAGING PHOTOMETER; OB1 MOLECULAR CLOUD; NGC 2264; INTERMEDIATE-MASS; DARK CLOUD; CLUSTER; PROTOCLUSTERS; OUTFLOWS; OBJECTS AB We analyze Spitzer and Magellan observations of a star-forming core near IRS 2 in the young cluster NGC 2264. The submillimeter source IRAS 12 S1, previously believed to be an intermediate-mass Class 0 object is shown to be a dense collection of embedded, low-mass stars. We argue that this group of stars represents the fragmenting collapse of a dense, turbulent core, using a number of indicators of extreme youth. With reasonable estimates for the velocity dispersion in the group, we estimate a dynamical lifetime of only a few times 10(4) yr. Spectral energy distributions of stars in the core are consistent with Class I or Class 0 assignments. We present observations of an extensive system of molecular hydrogen emission knots. The luminosity of the objects in the core region are consistent with roughly solar mass protostars. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Lisbon, Fac Ciencias, Dept Fis, Lisbon, Portugal. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Young, ET (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Teixeira, Paula Stella/O-2289-2013 OI Teixeira, Paula Stella/0000-0002-3665-5784 NR 27 TC 23 Z9 23 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP 972 EP 978 DI 10.1086/501227 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200030 ER PT J AU Prochaska, JX Bloom, JS Chen, HW Foley, RJ Perley, DA Ramirez-Ruiz, E Granot, J Lee, WH Pooley, D Alatalo, K Hurley, K Cooper, MC Dupree, AK Gerke, BF Hansen, BMS Kalirai, JS Newman, JA Rich, RM Richer, H Stanford, SA Stern, D van Breugel, WJM AF Prochaska, JX Bloom, JS Chen, HW Foley, RJ Perley, DA Ramirez-Ruiz, E Granot, J Lee, WH Pooley, D Alatalo, K Hurley, K Cooper, MC Dupree, AK Gerke, BF Hansen, BMS Kalirai, JS Newman, JA Rich, RM Richer, H Stanford, SA Stern, D van Breugel, WJM TI The galaxy hosts and large-scale environments of short-hard gamma-ray bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; stars : formation; stars : neutron ID STAR-FORMATION; SHORT-DURATION; FORMATION RATES; NEUTRON-STARS; GRB 050509B; AFTERGLOW; GRB-050709; REDSHIFT; CONSTRAINTS; RESOLUTION AB The rapid succession of discoveries of short-duration hard-spectrum gamma-ray bursts (GRBs) has led to unprecedented insights into the energetics of the explosion and nature of the progenitors. Yet short of the detection of a smoking gun, such as a burst of coincident gravitational radiation or a Li-Paczynski minisupernova, it is unlikely that a definitive claim can be made for the progenitors. As was the case with long-duration soft-spectrum GRBs, however, the expectation is that a systematic study of the hosts and locations of short GRBs could begin to yield fundamental clues as to their nature. We present an aggregate study of the host galaxies of short-duration hard-spectrum GRBs. In particular, we present the Gemini-North and Keck discovery spectra of the galaxies that hosted three short GRBs and a moderate-resolution ( R approximate to 6000) spectrum of a fourth host. We find that these short-hard GRBs originate in a variety of low-redshift (z < 1) environments that differ substantially from those of long-soft GRBs, both on individual galaxy scales and on galaxy-cluster scales. Specifically, three of the bursts are found to be associated with old and massive galaxies with no current (< 0.1 M-circle dot yr(-1)) or recent star formation. Two of these galaxies are located within a cluster environment. These observations support an origin from the merger of compact stellar remnants, such as double neutron stars or a neutron star-black hole binary. The fourth event, in contrast, occurred within a dwarf galaxy with a star formation rate exceeding 0.3 M-circle dot yr(-1). Therefore, it appears that like supernovae of Type Ia, the progenitors of short-hard bursts are created in all galaxy types, suggesting a corresponding class with a wide distribution of delay times between formation and explosion. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Inst Adv Study, Princeton, NJ 08540 USA. Stanford Univ, KIPAC, Stanford, CA 94309 USA. Natl Autonomous Univ Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Calif Berkeley, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Prochaska, JX (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. OI Alatalo, Katherine/0000-0002-4261-2326 NR 50 TC 73 Z9 73 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP 989 EP 994 DI 10.1086/501160 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200032 ER PT J AU Rana, VR Singh, KP Schlegel, EM Barrett, PE AF Rana, VR Singh, KP Schlegel, EM Barrett, PE TI Study of FeK alpha lines in nonmagnetic cataclysmic variables using Chandra HEG data SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; novae, cataclysmic variables; stars : individual (SS Cygni, SU Ursae Majoris, U Gemini, V426 Ophiuci, V603 Aquilae, WX Hydri); X-rays : stars ID XMM-NEWTON OBSERVATIONS; X-RAY OBSERVATIONS; DWARF NOVAE; SS-CYGNI; QUIESCENCE; OUTBURST; SPECTRA; IRON; SPECTROMETER; EVOLUTION AB Results from a study of Fe K alpha emission lines for a sample of six nonmagnetic cataclysmic variables (CVs) using high-resolution X-ray data from the Chandra High Energy Transmission Grating (HETG) are presented. Two of the sources, SS Cyg and U Gem, are observed in both quiescent and outburst states, whereas V603 Aql, V426 Oph, WXHyi, and SUUMa are observed only in quiescence. The fluorescent Fe line is prominent in V603 Aql, V426 Oph, and SS Cyg during quiescence, indicating the presence of a conspicuous reflection component in these sources. The observed equivalent width of the fluorescent Fe line is consistent with reflection from a white dwarf surface that subtends a 2 pi solid angle at the X-ray source. During the outburst in SS Cyg, the fluorescent line is redshifted by about 2300 km s(-1). The Fe xxv triplet at 6.7 keV is found to be dominant in all sources. The value of the G ratio derived from the Fe xxv triplet indicates that the plasma is in collisional ionization equilibrium during the quiescent state. The Fe xxv line is significantly broadened in U Gem and SS Cyg during the outbursts compared to quiescence, indicating the presence of high-velocity material near the white dwarf during the outburst. The ratio of Fe xxvi/xxv indicates a higher ionization temperature during quiescence than in outburst in U Gem and SS Cyg. C1 Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, EES Sci Software Grp, Baltimore, MD 21218 USA. RP Rana, VR (reprint author), Univ Texas, Dept Phys & Astron, 6900 N Loop 1604 W, San Antonio, TX 78249 USA. EM vrana@tifr.res.in; singh@tifr.res.in; eschlegel@cfa.harvard.edu; barrett@stsci.edu NR 32 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP 1042 EP 1050 DI 10.1086/500316 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200038 ER PT J AU Mackay, DH Ballegooijen, AA AF Mackay, D. H. van Ballegooijen, A. A. TI Models of the large-scale corona. II. Magnetic connectivity and open flux variation SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : magnetic fields ID LONG-TERM VARIATION; ACTIVE-REGION; HEMISPHERIC PATTERN; VECTOR MAGNETOGRAMS; FILAMENT FORMATION; MASS EJECTIONS; FIELDS; EVOLUTION; SUN; ROPES AB In this paper the changing connectivity of the coronal magnetic field during the formation and ejection of magnetic flux ropes is considered. Using recent simulations of the coronal field, it is shown that reconnection may occur both above and below the flux ropes. Those occurring above slowly strip away coronal arcades overlying the flux ropes and allow the flux ropes to be ejected. In contrast, those below help to push the flux ropes out. It is found that the reconnection occurring below each flux rope may result in significant skew being maintained within the coronal field above the PIL after the flux rope is ejected. In addition, after the eruption, as the coronal field closes down, the large-scale transport of open flux across the bipoles takes place through the process of "interchange reconnection.'' As a result, new photospheric domains of open flux are created within the centers of the bipoles, where field lines were previously closed. The net open flux in the simulation may be split into two distinct contributions. The first contribution is due to the nonpotential equilibrium coronal fields of the bipoles. The second contribution is a temporary enhancement to this during the ejection of the flux ropes, where previously closed field lines become open. It is shown that the nonpotential equilibrium contribution to the open flux is significantly higher than that due to a potential field deduced from the same photospheric boundary conditions. These results suggest that the nonpotential nature of coronal magnetic fields may affect the variation of the Sun's open flux during periods of high solar activity and should be considered in future simulations. C1 Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM duncan@mcs.st-and.ac.uk; vanballe@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 62 TC 37 Z9 38 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 MAY 10 PY 2006 VL 642 IS 2 BP 1193 EP 1204 DI 10.1086/501043 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UC UT WOS:000237554200051 ER PT J AU Aerts, C De Cat, P Kuschnig, R Matthews, JM Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH Weiss, WW AF Aerts, C De Cat, P Kuschnig, R Matthews, JM Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH Weiss, WW TI Discovery of the new slowly pulsating B star HD 163830 (B5 II/III) from MOST space-based photometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : early-type; stars : fundamental parameters; stars : individual (HD 163830); stars : oscillations; stars : rotation ID GAMMA-DORADUS STARS; G-MODES AB We report the discovery of a new slowly pulsating B star, with the largest number of detected frequencies to date by more than a factor of 3, based on 37 days of MOST (Microvariability and Oscillations of STars) satellite guide star photometry. The star HD 163830 (V = 9.3, B5 II/III) varies in 20 detected frequencies in the range 0.035-1.06 day(-1) (0.4-12.3 mu Hz) with amplitudes from 0.7 to 7.6 mmag (with a signal-to-noise ratio from 4 to 41). Eighteen of these frequencies are consistent with low-degree, high-order nonradial g-modes of seismic models of an evolved 4.5 M-circle dot star. We are unable to identify one unique model due to lack of mode identifications. The lowest two frequencies may be associated with the rotation of HD 163830, but firm proof of this must await future spectroscopic data. C1 Univ Louvain, Inst Astron, B-3001 Louvain, Belgium. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL0 Nijmegen, Netherlands. Royal Observ Belgium, B-1180 Brussels, Belgium. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Aerts, C (reprint author), Univ Louvain, Inst Astron, Celestijnenlaan 200B, B-3001 Louvain, Belgium. EM conny@ster.kuleuven.be NR 21 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L165 EP L168 DI 10.1086/504634 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300020 ER PT J AU Borkowski, KJ Williams, BJ Reynolds, SP Blair, WP Ghavamian, P Sankrit, R Hendrick, SP Long, KS Raymond, JC Smith, RC Points, S Winkler, PF AF Borkowski, KJ Williams, BJ Reynolds, SP Blair, WP Ghavamian, P Sankrit, R Hendrick, SP Long, KS Raymond, JC Smith, RC Points, S Winkler, PF TI Dust destruction in type Ia supernova remnants in the large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; Magellanic Clouds; supernova remnants ID NONRADIATIVE SHOCKS; INFRARED-EMISSION; SMALL GRAINS; BLAST WAVES; PHYSICS; EJECTA AB We present first results from an extensive survey of Magellanic Cloud supernova remnants (SNRs) with the Spitzer Space Telescope. We describe IRAC and MIPS imaging observations at 3.6, 4.5, 5.8, 8, 24, and 70 mu m of four Balmer-dominated Type Ia SNRs in the Large Magellanic Cloud (LMC): DEM L71 (0505-67.9), 0509-67.5, 0519-69.0, and 0548-70.4. None was detected in the four short- wavelength IRAC bands, but all four were clearly imaged at 24 mm, and two at 70 mm. A comparison of these images with Chandra broadband X-ray images shows a clear association with the blast wave, and not with internal X-ray emission associated with ejecta. Our observations are well described by one-dimensional shock models of collisionally heated dust emission, including grain size distributions appropriate for the LMC, grain heating by collisions with both ions and electrons, and sputtering of small grains. Model parameters are constrained by X-ray, optical, and far-ultraviolet observations. Our models can reproduce observed 70/24 mu m flux ratios only by including sputtering, destroying most grains smaller than 0.03-0.04 mu m in radius. We infer total dust masses swept up by the SNR blast waves, before sputtering, on the order of 10(-2) M-circle dot, several times less than those implied by a dust-to-gas mass ratio of 0.3% as often assumed for the LMC. Substantial dust destruction has implications for gas-phase abundances. C1 N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Borkowski, KJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. EM kborkow@ncsu.edu NR 30 TC 52 Z9 52 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L141 EP L144 DI 10.1086/504472 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300014 ER PT J AU Holden, BP Franx, M Illingworth, GD Postman, M Blakeslee, JP Homeier, N Demarco, R Ford, HC Rosati, P Kelson, DD Tran, KVH AF Holden, BP Franx, M Illingworth, GD Postman, M Blakeslee, JP Homeier, N Demarco, R Ford, HC Rosati, P Kelson, DD Tran, KVH TI The possible z=0.83 precursors of z=0, M* early-type cluster galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (MS 1054.4-0321, Cl 0152.7-1357); galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : fundamental parameters ID MORPHOLOGY-DENSITY RELATION; COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT CLUSTERS; FUNDAMENTAL-PLANE; INTERMEDIATE-REDSHIFT; LUMINOSITY FUNCTIONS; COMA CLUSTER; EVOLUTION; POPULATION; Z-SIMILAR-OR-EQUAL-TO-1 AB We examine the distribution of stellar masses of galaxies in MS 1054.4 - 0321 and Cl 0152.7 - 1357, two X-ray-selected clusters of galaxies at z = 0.83. Our stellar mass estimates, from spectral energy distribution fitting, reproduce the dynamical masses as measured from velocity dispersions and half-light radii with a scatter of 0.2 dex in the mass for early-type galaxies. When we restrict our sample of members to high stellar masses, those over 10(11.1) M-circle dot (M* in the Schechter mass function for cluster galaxies), we find that the fraction of early-type galaxies is 79% +/- 6% at z = 0.83 and 87% +/- 6% at z = 0.023 for the Coma Cluster, consistent with no evolution. Previous work with luminosity-selected samples has found that the early-type fraction in rich clusters declines from similar or equal to 80% at z = 0 to similar or equal to 60% at z = 0.8. The observed evolution in the early-type fraction from luminosity-selected samples must predominantly occur among sub-M* galaxies. As M* for field and group galaxies, especially late types, is below M* for cluster galaxies, infall could explain most of the recent growth in the early-type fraction. Future surveys could determine the morphological distributions of lower mass systems, which would confirm or refute this explanation. C1 Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95065 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Holden, BP (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, 1156 High St, Santa Cruz, CA 95065 USA. EM holden@ucolick.org OI Blakeslee, John/0000-0002-5213-3548 NR 35 TC 21 Z9 21 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L123 EP L126 DI 10.1086/504714 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300010 ER PT J AU Narayanan, D Cox, TJ Robertson, B Dave, R Di Matteo, T Hernquist, L Hopkins, P Kulesa, C Walker, CK AF Narayanan, Desika Cox, Thomas J. Robertson, Brant Dave, Romeel Di Matteo, Tiziana Hernquist, Lars Hopkins, Philip Kulesa, Craig Walker, Christopher K. TI Molecular outflows in galaxy merger simulations with embedded active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; galaxies : formation; galaxies : interactions; galaxies : ISM; line : formation ID ULTRALUMINOUS INFRARED GALAXIES; QUASAR LUMINOSITY FUNCTION; STAR-FORMING GALAXIES; BLACK-HOLES; SUBMILLIMETER GALAXIES; ELLIPTIC GALAXIES; CO OBSERVATIONS; GAS; STARBURSTS; EVOLUTION AB We study the effects of feedback from active galactic nuclei (AGNs) on emission from molecular gas in galaxy mergers by combining hydrodynamic simulations that include black holes with a three-dimensional, non-local thermodynamic equilibrium (LTE) radiative transfer code. We find that molecular clouds entrained in AGN winds produce an extended CO morphology with significant off-nuclear emission, which may be detectable via contour mapping. Furthermore, kinematic signatures of these molecular outflows are visible in emission-line profiles when the outflow has a large line-of-sight velocity. Our results can help interpret current and upcoming observations of luminous infrared galaxies, as well as provide a detailed test of subresolution prescriptions for supermassive black hole growth in galaxy-scale hydrodynamic simulations. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Narayanan, D (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM dnarayanan@as.arizona.edu RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 52 TC 37 Z9 37 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L107 EP L110 DI 10.1086/504846 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300006 ER PT J AU Sasaki, M Kothes, R Plucinsky, PP Gaetz, TJ Brunt, CM AF Sasaki, M Kothes, R Plucinsky, PP Gaetz, TJ Brunt, CM TI Evidence for shocked molecular gas in the Galactic supernova remnant CTB 109 (G109.1-1.0) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; shock waves; supernova remnants; X-rays : individual (CTB 109) ID CLOUDS; RATIO AB We report the detection of molecular clouds around the X-ray-bright interior feature in the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0). This feature, called the "lobe," has been previously suggested to be the result of an interaction of the SNR shock wave with a molecular cloud complex. We present new high-resolution X-ray data from the Chandra X-Ray Observatory and new high-resolution CO data from the Five College Radio Astronomy Observatory that show the region of interaction with the cloud complex in greater detail. The CO data reveal three clouds around the lobe in the velocity interval. The velocity -57 km s(-1) < v < -52 km s(-1) profiles of (CO)-C-12 in various parts of the east cloud are well fit with a Gaussian; however, at the position at which the CO cloud and the lobe overlap, the velocity profile has an additional component toward higher negative velocities. The molecular hydrogen density in this part of the cloud is relatively high (N-H2 approximate to 1.9 x 10(20) cm(-2)), whereas the foreground absorption in X-rays (NH approximate to 4.5 x 10(21) cm(-2)), obtained from Chandra data, is lower than in other parts of the cloud and in the north and south clouds. These results indicate that the east cloud has been hit by the SNR blast wave on the western side, forming the bright X- ray lobe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Domin Radio Astrophys Observ, Herzberg Inst Astrophys, Natl Res Council Canada, Penticton, BC V2A 6J9, Canada. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. RP Sasaki, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msasaki@cfa.harvard.edu; roland.kothes@nrc-cnrc.gc.ca; pplucinsky@cfa.harvard.edu; brunt@astro.ex.ac.uk RI Sasaki, Manami/P-3045-2016 OI Sasaki, Manami/0000-0001-5302-1866 NR 16 TC 13 Z9 13 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L149 EP L152 DI 10.1086/504844 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300016 ER PT J AU Williams, RJ Mathur, S Nicastro, F Elvis, M AF Williams, RJ Mathur, S Nicastro, F Elvis, M TI XMM-Newton view of the z > 0 warm-hot intergalactic medium toward Markarian 421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; intergalactic medium; X-rays : general ID X-RAY FOREST; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; ABSORPTION-LINE SYSTEMS; LOW-REDSHIFT; CHANDRA DETECTION; SIGHT LINE; LY-ALPHA; BARYONS AB The recent detection with Chandra of two warm-hot intergalactic medium (WHIM) filaments toward Mrk 421 by Nicastro et al. provides a measurement of the bulk of the "missing baryons" in the nearby universe. Since Mrk 421 is a bright X-ray source, it is also frequently observed by the XMM-Newton Reflection Grating Spectrometer (RGS) for calibration purposes. Using all available archived XMM observations of this source with small pointing offsets (< 15"), we construct the highest quality XMM grating spectrum of Mrk 421 to date with a net exposure time (excluding periods of high background flux) of 437 ks and similar to 15,000 counts per resolution element at 21.6 angstrom more than twice that of the Chandra spectrum. Despite the long-exposure time, neither of the two intervening absorption systems is seen, although the upper limits derived are consistent with the Chandra equivalent width measurements. This appears to result from (1) the larger number of narrow instrumental features caused by bad detector columns, (2) the degraded resolution of XMM/RGS as compared to the Chandra/LETG, and (3) fixed-pattern noise at lambda greater than or similar to 29 angstrom. The nondetection of the WHIM absorbers by XMM is thus fully consistent with the Chandra measurement. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Italy. RP Williams, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18Th Ave, Columbus, OH 43210 USA. NR 20 TC 17 Z9 17 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2006 VL 642 IS 2 BP L95 EP L98 DI 10.1086/504635 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042UD UT WOS:000237554300003 ER PT J AU Reinert, JF Harbach, RE AF Reinert, JF Harbach, RE TI Descriptions of genus Downsiomyia Vargas (Diptera : Culicidae : Aedini) and its type species Do. nivea (Ludlow) SO ZOOTAXA LA English DT Review DE Aedes; Downsiomyia; Finlaya; Albonivea Group; Nivea Group; Do. nivea; mosquitoes ID MOSQUITOS DIPTERA; WUCHERERIA-BANCROFTI; SYNOPTIC CATALOG; PUBLIC-HEALTH; INDIA DIPTERA; AEDES; TRANSMISSION; INDONESIA; ISLANDS; CLASSIFICATION AB Genus Downsiomyia and its type species, Do. nivea (Ludlow), are described in detail. The 30 species included in the genus are listed. An extensive list of previous literature pertaining to the genus is provided. C1 ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL 32608 USA. Natl Museum Nat Hist, Walter Reed Biosystemat Unit, Smithsonian Inst, Washington, DC 20560 USA. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. RP Reinert, JF (reprint author), ARS, Ctr Med Agr & Vet Entomol, USDA, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. EM jreinert@gainesville.usda.ufl.edu; r.harbach@nhm.ac.uk NR 248 TC 3 Z9 3 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 MAY 8 PY 2006 IS 1196 BP 33 EP 61 PG 29 WC Zoology SC Zoology GA 040DC UT WOS:000237358200002 ER PT J AU Staines, CL AF Staines, CL TI A new combination and two new species of Aslamidium Borowiec (Coleoptera : Chrysomelidae : Cassidinae) SO ZOOTAXA LA English DT Article DE Aslamidium; Chrysomelidae; Cassidinae; new species AB Aslamidium ( Neoaslamidium) flavomaculata from Colombia, Ecuador, and Panama and A. (N.) lepidum from Colombia are described as new and illustrated. Demotispa strandi Uhmann is transferred to Aslamidium ( Neoaslamidium) and is reported for the first time from Panama. A key to the known species of Aslamidium is presented. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu NR 14 TC 3 Z9 3 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 8 PY 2006 IS 1195 BP 61 EP 68 PG 8 WC Zoology SC Zoology GA 040DB UT WOS:000237358100004 ER PT J AU Gridi-Papp, M Rand, AS Ryan, MJ AF Gridi-Papp, M Rand, AS Ryan, MJ TI Animal communication: Complex call production in the tungara frog SO NATURE LA English DT Article ID PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; MORPHOLOGY; SYRINX C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Univ Estadual Paulista, Inst Biociencias, Dept Zool, BR-13506900 Sao Paulo, Brazil. RP Gridi-Papp, M (reprint author), Univ Calif Los Angeles, Dept Physiol Sci, Los Angeles, CA 90095 USA. EM mryan@mail.utexas.edu NR 10 TC 48 Z9 49 U1 2 U2 22 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 4 PY 2006 VL 441 IS 7089 BP 38 EP 38 DI 10.1038/441038a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 038TB UT WOS:000237248600025 PM 16672962 ER PT J AU Volkov, I Banavar, JR He, FL Hubbell, SP Maritan, A AF Volkov, I Banavar, JR He, FL Hubbell, SP Maritan, A TI Theoretical biology - Comparing models of species abundance - Reply SO NATURE LA English DT Letter C1 Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. Penn State Univ, Ctr Infect Dis Dynam, Dept Biol, University Pk, PA 16802 USA. Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. RP Volkov, I (reprint author), Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. EM jayanth@phys.psu.edu NR 3 TC 4 Z9 4 U1 3 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 4 PY 2006 VL 441 IS 7089 BP E1 EP E2 DI 10.1038/nature04827 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 038TB UT WOS:000237248600027 ER PT J AU Conn, JE Vineis, JH Bollback, JP Onyabe, DY AF Conn, Jan E. Vineis, Joseph H. Bollback, Jonathan P. Onyabe, David Y. TI Population structure of the malaria vector Anopheles darlingi in a malaria-endemic region of eastern Amazonian Brazil SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID GENETIC DIFFERENTIATION; PLASMODIUM-FALCIPARUM; SOUTH-AMERICA; MICROSATELLITE LOCI; WEST-AFRICA; MITOCHONDRIAL-DNA; DIRUS MOSQUITOS; F-STATISTICS; SAO-TOME; GAMBIAE AB Anopheles darlingi is the primary malaria vector in Latin America, and is especially important in Amazonian Brazil. Historically, control efforts have been focused on indoor house spraying using a variety of insecticides, but since the mid-1990s there has been a shift to patient treatment and focal insecticide fogging. Anopheles darlingi was believed to have been significantly reduced in a gold-mining community, Peixoto de Azevedo (in Mato Grosso State), in the early 1990s by insecticide use during a severe malaria epidemic. In contrast, although An. darlingi was eradicated from some districts of the city of Belem (the capital of Para State) in 1968 to reduce malaria, populations around the water protection area in the eastern district were treated only briefly. To investigate the population structure of An. darlingi including evidence for a population bottleneck in Peixoto, we analyzed eight microsatellite loci of 256 individuals from seven locations in Brazil: three in Amapa State, three in Para State, and one in Mato Grosso State. Allelic diversity and mean expected heterozygosity were high for all populations (mean number alleles/locus and H(E) were 13.5 and 0.834, respectively) and did not differ significantly between locations. Significant heterozygote deficits were associated with linkage disequilibrium, most likely due to either the Wahlund effect or selection. We found no evidence for a population bottleneck in Peixoto, possibly because the reduction was not extreme enough to be detected. Overall estimates of long-term N(e) varied from 92.4 individuals under the linkage disequilibrium model to infinity under the heterozygote excess model. Fixation indices and analysis of molecular variance demonstrated significant differentiation between locations north and south of the Amazon River, suggesting a degree of genetic isolation between them, attributed to isolation by distance. C1 New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA. Univ Vermont, Dept Biol, Burlington, VT USA. Univ Copenhagen, Ctr Bioinformat, Copenhagen, Denmark. Aeras Global TB Vaccine Fdn, Rockville, MD USA. Walter Reed Army Inst Res, Museum Support Ctr, Smithsonian Inst, Suitland, MD USA. Inst Evandro Chagas, Ananindeua, Para, Brazil. RP Conn, JE (reprint author), New York State Dept Hlth, Wadsworth Ct, Griffin Lab, 5668 State Farm Rd, Slingerlands, NY 12159 USA. EM jconn@wadsworth.org OI Conn, Jan/0000-0002-5301-7020 FU NIAID NIH HHS [R01 AI054139, AI R2940116, AI R0154139] NR 83 TC 28 Z9 30 U1 1 U2 2 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 MAY PY 2006 VL 74 IS 5 BP 798 EP 806 PG 9 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 041GA UT WOS:000237441100020 PM 16687683 ER PT J AU Kitchen, AM Gese, EM Waits, LP Karki, SM Schauster, ER AF Kitchen, Ann M. Gese, Eric M. Waits, Lisette P. Karki, Seija M. Schauster, Edward R. TI Multiple breeding strategies in the swift fox, Vulpes velox SO ANIMAL BEHAVIOUR LA English DT Article ID EXTRA-PAIR PATERNITY; HOME-RANGE; SOUTHEASTERN COLORADO; SPATIAL-ORGANIZATION; SOCIAL-BEHAVIOR; GRAY SEAL; ECOLOGY; LIKELIHOOD; MONOGAMY; COYOTES AB Little is known of the mating system of the swift fox or how it compares to other socially monogamous mammals. In a 4-year study of 188 swift foxes, we used microsatellite analysis at 11 loci along with spatial observations to investigate swift fox mating strategies. The mating strategies used by swift foxes were highly diverse. Previous field observations have indicated that the swift fox is socially monogamous. However, we found that extrapair mating was a common breeding strategy; 52% of offspring were sired by a male that was not the mate of their mother. There was also variation in the structure of social groups. Of 59 social groups, the most common consisted of a male and female pair (93% of social groups); however, four stable trios of both one female and two males (5%) and two females and one male (2%) were also evident. The trio groups were spatially associated, and at least one member of each trio was highly related to a member in at least one other trio. Swift foxes also engaged in mate switching, which refutes the prevailing hypothesis that they always mate for life. Thus, we found that the mating system of the swift fox is highly diverse and substantially more complex than previously believed. We discuss factors that may influence which strategies are adopted and whether they are adaptive. (c) 2006 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 Utah State Univ, Dept Forest Range & Wildlife Sci, Logan, UT 84322 USA. Utah State Univ, Natl Wildlife Res Ctr, USDA, Wildlife Serv,Dept Forest Range & Wildlife Sci, Logan, UT 84322 USA. Univ Idaho, Dept Fish & Wildlife Resources, Moscow, ID 83843 USA. RP Kitchen, AM (reprint author), Smithsonian Inst, Monitoring & Assessment Biodivers Program, NZP, CRC,MRC 705,POB 37012, Washington, DC 20013 USA. EM hendersonan@si.edu RI Gese, Eric/B-4578-2011 NR 68 TC 32 Z9 34 U1 2 U2 27 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 MAY PY 2006 VL 71 BP 1029 EP 1038 DI 10.1016/j.anbehav.2005.06.015 PN 5 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 050SN UT WOS:000238108600004 ER PT J AU Kirkpatrick, M Rand, AS Ryan, MJ AF Kirkpatrick, Mark Rand, A. Stanley Ryan, Michael J. TI Mate choice rules in animals SO ANIMAL BEHAVIOUR LA English DT Article ID SENSITIVE FORAGING PREFERENCES; JAYS PERISOREUS-CANADENSIS; ROCK-PAPER-SCISSORS; SEXUAL SELECTION; FEMALE CHOICE; MATING PREFERENCES; TUNGARA FROG; INTRANSITIVITY; EVOLUTION; MODELS AB We identify several fundamental properties of how females choose mates and propose statistical methods to test hypotheses about them. Virtually, all studies of mate choice have implicitly assumed that choice involves what we call strict preference. By that we mean that all the properties of a stimulus can be reduced to a single preference value that is independent of other stimuli, and that the stronger a female's preference for a male, the more likely she is to choose him. An important consequence of strict preference is that it guarantees that females cannot show intransitive choice (where male X-1 is preferred over male X-2, and X-2 over X-3, but X-3 is preferred over X-1). We find general conditions for the strict preference paradigm to apply in the simple situation where females choose between two potential mates. We illustrate how these conditions can be tested statistically using data on mate choice in tungara frogs, Physalaemus pustulosus. The results were not consistent with any of the standard models for strict preference. On the other hand, we also failed to find statistical support for intransitive choice. We suggest that understanding mate choice will require deeper analysis of the most basic properties of the choice rules. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Kirkpatrick, M (reprint author), Univ Texas, Sect Integrat Biol, 1 Univ Stn C-0930, Austin, TX 78712 USA. EM kirkp@mail.utexas.edu NR 44 TC 38 Z9 38 U1 0 U2 17 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 MAY PY 2006 VL 71 BP 1215 EP 1225 DI 10.1016/j.anbehav.2005.11.010 PN 5 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 050SN UT WOS:000238108600025 ER PT J AU Christy, JH Backwell, PRY AF Christy, John H. Backwell, Patricia R. Y. TI No preference for exaggerated courtship signals in a sensory trap SO ANIMAL BEHAVIOUR LA English DT Article ID MALE FIDDLER-CRABS; SEXUAL SELECTION; RECEIVER BIASES; PILLAR FUNCTION; UCA-MUSICA; ATTRACTIVENESS; HYPOTHESIS; RESOLUTION; EVOLUTION; HORIZON AB Courting male fiddler crabs, Uca terpsichores, construct unusually large sand hoods at the entrances to their burrows to which they attract females for mating. Females sequentially visit several courting males before they stay with one and mate in his burrow, and they preferentially approach burrows with hoods. While moving between burrows, crabs are at risk of predation by birds and they sometimes run to objects that provide temporary cover. Thus, the female preference for burrows with hoods may help females to avoid predators. Could selection for predator avoidance produce a directional preference for especially large hoods? To examine this possibility, we made multiple replicas of two kinds of hood models with exaggerated dimensions (super models and wall models) and a single model with average dimensions (average models). Super models were four standard deviations taller and two standard deviations wider than average-size natural hoods. Wall models were of average height but near the maximum width of natural hoods; when males 'overbuild', they construct wall-like hoods. We replaced males' hoods with these models and measured their effects on male attractiveness. Males with exaggerated models neither encountered nor attracted more females than did males with average models or natural hoods. Females did not show a directional preference for larger hoods. The attractiveness of hoods may plateau with increasing size because discrimination between average and larger hoods may result in fatal hesitation, preventing the evolution of a directional preference for an exaggerated form of this courtship signal. Males build hoods from pure sand, so males may build unusually large hoods because they are more durable, not because they are better signals. C1 Smithsonian Trop Res Inst, Balboa, Panama. Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM christyj@si.edu RI Backwell, Patricia/C-8883-2009 NR 40 TC 11 Z9 12 U1 2 U2 6 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 MAY PY 2006 VL 71 BP 1239 EP 1246 DI 10.1016/j.anbehav.2005.11.008 PN 5 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 050SN UT WOS:000238108600027 ER PT J AU Zotz, G Richter, A AF Zotz, G Richter, A TI Changes in carbohydrate and nutrient contents throughout a reproductive cycle indicate that phosphorus is a limiting nutrient in the epiphytic bromeliad, Werauhia sanguinolenta SO ANNALS OF BOTANY LA English DT Article DE Barro Colorado Island; Bromeliaceae; cost of reproduction; nitrogen; non-structural carbohydrates; nutrient uptake; phosphorus; reproductive investment; seeds; Werauhia sanguinolenta ID DIMERANDRA-EMARGINATA; VASCULAR EPIPHYTES; MINERAL-NUTRITION; FRUIT PRODUCTION; TROPICAL FOREST; PLANTS; ORCHID; LIMITATION; ALLOCATION; PHOTOSYNTHESIS AB Background and Aims This study examined the physiological basis of the cost of reproduction in the epiphytic bromeliad Werauhia sanguinolenta, growing in situ in a tropical lowland forest in Panama. Methods Entire mature plants were sampled repeatedly over the course of 2 years, which represents the common interval between reproductive events. Due to the uncertainty concerning the appropriate currency of resource allocation to reproduction, the temporal changes of the contents of total non-structural carbohydrates (TNC) and of all major nutrient elements in different plant parts were studied (stems, green leaves, non-green leaf bases, roots and reproductive structures when present). Key Results Although TNC varied with time in all compartments, this variation was more related to seasonal fluctuations than to reproductive status. The contents of the nutrient elements, N, P, K, Mg and S, on the other hand, showed significant differences between reproductive and non-reproductive individuals, while Ca did not change with reproductive status. Differences in nutrient contents were most pronounced in stems. Seeds were particularly enriched in P, much less so in N and the other nutrient elements. Model calculations of nutrient fluxes indicate that a plant needs about 2 years to accumulate the amount of P invested in a fruit crop, while the estimated uptake rates for N were much faster. Conclusions Since most mature individuals of this species fruit every other year, it is hypothesized that P is the prime limiting factor for reproduction. These findings therefore add to an increasing body of evidence that P rather than N is limiting growth and reproduction in vascular epiphytes. C1 Univ Basel, Bot Inst, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Vienna, Dept Chem Ecol & Ecosyst Res, A-1090 Vienna, Austria. RP Zotz, G (reprint author), Univ Basel, Bot Inst, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch RI Richter, Andreas/D-8483-2012 OI Richter, Andreas/0000-0003-3282-4808 NR 44 TC 22 Z9 24 U1 0 U2 16 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 MAY PY 2006 VL 97 IS 5 BP 745 EP 754 DI 10.1093/aob/mcl026 PG 10 WC Plant Sciences SC Plant Sciences GA 035JP UT WOS:000236997400008 PM 16497701 ER PT J AU Lacy, CHS Torres, G Claret, A Menke, JL AF Lacy, CHS Torres, G Claret, A Menke, JL TI Absolute properties of the main-sequence eclipsing binary star EY Cephei SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : evolution; stars : fundamental parameters; stars : individual (EY Cephei) ID LIMB-DARKENING COEFFICIENTS; SYNCHRONIZATION TIMES; CHEMICAL-COMPOSITION; TIDAL-EVOLUTION; LIGHT CURVES; CIRCULARIZATION; SYSTEMS AB We present 6907 differential photometric observations in the V filter, as well as 52 radial velocities from spectroscopic observations of the detached, eccentric 7.97 day double-lined eclipsing binary star EY Cep. Absolute dimensions of the components are determined with high precision ( less than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.523 +/- 0.008 M-circle dot and 1.463 +/- 0.010 R-circle dot for the primary and 1.498 +/- 0.014 M-circle dot and 1.468 +/- 0.010 R-circle dot for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from the spectra, uvby beta, and UBV photometry: 7090 +/- 150 K for the primary and 6970 +/- 150 K for the secondary, corresponding to spectral types of F0 and F0, and 0.036 mag for the color excess Eb-y. Spectral line widths give rotational velocities that are synchronous with the mean orbital motion in a highly eccentric orbit (e = 0.4429). The components of EY Cep are young main-sequence stars with an age of about 40 million years, according to models. C1 Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Menke Sci Ltd, Bamesville, MD 20838 USA. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM clacy@uark.edu; gtorres@cfa.harvard.edu; claret@iaa.es; john@menkescientific.com NR 34 TC 5 Z9 6 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2006 VL 131 IS 5 BP 2664 EP 2672 DI 10.1086/501527 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 037KY UT WOS:000237146900028 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, BC Kenyon, SJ TI A hybrid N-body-coagulation code for planet formation SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID EARLY KUIPER-BELT; SYMPLECTIC INTEGRATORS; ACCRETIONAL EVOLUTION; COLLISIONAL CASCADES; TERRESTRIAL PLANETS; VELOCITY EVOLUTION; OLIGARCHIC GROWTH; TIDAL INTERACTION; RUNAWAY GROWTH; BETA-PICTORIS AB We describe a hybrid algorithm to calculate the formation of planets from an initial ensemble of planetesimals. The algorithm uses a coagulation code to treat the growth of planetesimals into oligarchs and explicit N-body calculations to follow the evolution of oligarchs into planets. To validate the N-body portion of the algorithm, we use a battery of tests in planetary dynamics. Several complete calculations of terrestrial planet formation with the hybrid code yield good agreement with previously published calculations. These results demonstrate that the hybrid code provides an accurate treatment of the evolution of planetesimals into planets. C1 Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys, 201 JFB, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 66 TC 49 Z9 49 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2006 VL 131 IS 5 BP 2737 EP 2748 DI 10.1086/503280 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 037KY UT WOS:000237146900036 ER PT J AU Tozzi, P Gilli, R Mainieri, V Norman, C Risaliti, G Rosati, P Bergeron, J Borgani, S Giacconi, R Hasinger, G Nonino, M Streblyanska, A Szokoly, G Wang, JX Zheng, W AF Tozzi, P Gilli, R Mainieri, V Norman, C Risaliti, G Rosati, P Bergeron, J Borgani, S Giacconi, R Hasinger, G Nonino, M Streblyanska, A Szokoly, G Wang, JX Zheng, W TI X-ray spectral properties of active galactic nuclei in the Chandra Deep Field South SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE x-rays : diffuse background; surveys; cosmology : observations; X-rays : galaxies; galaxies : active ID XMM-NEWTON OBSERVATION; STAR-FORMING GALAXIES; NORTH SURVEY; NUMBER COUNTS; SEYFERT-GALAXIES; LOCKMAN-HOLE; IMAGING SPECTROMETER; LUMINOSITY FUNCTION; HELLAS2XMM SURVEY; SYNTHESIS MODELS AB We present a detailed X-ray spectral analysis of the sources in the 1Ms catalog of the Chandra Deep Field South ( CDFS) taking advantage of optical spectroscopy and photometric redshifts for 321 extragalactic sources out of the total sample of 347 sources. As a default spectral model, we adopt a power law with slope Gamma with an intrinsic redshifted absorption N-H, a fixed Galactic absorption and an unresolved Fe emission line. For 82 X-ray bright sources, we are able to perform the X-ray spectral analysis leaving both Gamma and N-H free. The weighted mean value for the slope of the power law is similar or equal to 1.75 +/- 0.02, and the distribution of best fit values shows an intrinsic dispersion of sigma(int) similar or equal to 0.30. We do not find hints of a correlation between the spectral index Gamma and the intrinsic absorption column density N-H. We then investigate the absorption distribution for the whole sample, deriving the N-H values in faint sources by fixing Gamma = 1.8. We also allow for the presence of a scattered component at soft energies with the same slope of the main power law, and for a pure reflection spectrum typical of Compton-thick AGN. We detect the presence of a scattered soft component in 8 sources; we also identify 14 sources showing a reflection-dominated spectrum. The latter are referred to as Compton-thick AGN candidates. By correcting for both incompleteness and sampling-volume effects, we recover the intrinsic N-H distribution representative of the whole AGN population, f ( N-H) dN(H), from the observed one. f ( N-H) shows a lognormal shape, peaking around log( N-H) similar or equal to 23.1 and with sigma similar or equal to 1.1. Interestingly, such a distribution shows continuity between the population of Compton-thin and that of Compton-thick AGN. We find that the fraction of absorbed sources ( with N-H > 10(22) cm(-2)) in the sample is constant ( at the level of about 75%) or moderately increasing with redshift. Finally, we compare the optical classification to the X-ray spectral properties, confirming that the correspondence of unabsorbed ( absorbed) X-ray sources to optical type I ( type II) AGN is accurate for at least 80% of the sources with spectral identification ( 1/3 of the total X-ray sample). C1 Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. Inst Astrophys, F-75014 Paris, France. Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy. Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. RP Tozzi, P (reprint author), Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34131 Trieste, Italy. OI Risaliti, Guido/0000-0002-3556-977X; Nonino, Mario/0000-0001-6342-9662; Borgani, Stefano/0000-0001-6151-6439 NR 95 TC 247 Z9 248 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 MAY PY 2006 VL 451 IS 2 BP 457 EP U60 DI 10.1051/0004-6361:20042592 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039AP UT WOS:000237272100013 ER PT J AU Dennerl, K Lisse, CM Bhardwaj, A Burwitz, V Englhauser, J Gunell, H Holmstrom, M Jansen, F Kharchenko, V Rodriguez-Pascual, PM AF Dennerl, K Lisse, CM Bhardwaj, A Burwitz, V Englhauser, J Gunell, H Holmstrom, M Jansen, F Kharchenko, V Rodriguez-Pascual, PM TI First observation of Mars with XMM-Newton - High resolution X-ray spectroscopy with RGS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic processes; molecular processes; solar wind; sun : X-rays, gamma rays; planets and satellites : individual : Mars; X-rays : individuals : Mars ID WIND CHARGE-EXCHANGE; SOLAR-WIND; PARAMETER-ESTIMATION; EMISSION; SPECTRA; VENUS; DISCOVERY; CHANDRA; HELIUM; COMETS AB In the first observation of Mars with XMM-Newton, on 20-21 November 2003, this planet is clearly detected as an X-ray source. High resolution X-ray spectroscopy with the Reflection Grating Spectrometer (RGS) confirms that the X-ray radiation from Mars is composed of two different components: one due to fluorescent scattering of solar X-rays in its upper atmosphere and the other one due to solar wind charge exchange in its exosphere. Close to Mars, the RGS spectrum is dominated by two pronounced CO2 fluorescence lines at 23.5 angstrom and 23.7 angstrom. Fluorescence from N-2 at 31.5 angstrom is also observed. With increasing distance from Mars, these lines fade, while numerous (similar to 12) emission lines become prominent at the positions expected for de-excitation of highly ionized C, N, O, and Ne atoms, strongly resembling a cometary X-ray spectrum. The He-like O6+ multiplet is resolved and is dominated by the spin-forbidden magnetic dipole transition 2 S-3(1) -> 1 S-1(0), confirming charge exchange as the origin of the emission, while the resonance line 2 P-1(1) -> 1 S-1(0) increases in intensity closer to Mars, where the density of the exosphere is higher. The high spectral dispersion and throughput of XMM-Newton / RGS make it possible to produce X- ray images of the Martian exosphere in individual emission lines, free from fluorescent radiation. They show extended emission out to similar to 8 Mars radii, with morphological differences between individual ions and ionization states. This is the first definite detection of charge exchange induced X-ray emission from the exosphere of another planet, providing a direct link to cometary X- ray emission. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Swedish Inst Space Phys, S-98128 Kiruna, Sweden. European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. XMM Newton SOC, Madrid 28080, Spain. RP Dennerl, K (reprint author), Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. EM kod@mpe.mpg.de RI Gunell, Herbert/D-5611-2013; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Gunell, Herbert/0000-0001-5379-1158; Bhardwaj, Anil/0000-0003-1693-453X NR 36 TC 56 Z9 56 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2006 VL 451 IS 2 BP 709 EP 722 DI 10.1051/0004-6361:20054253 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039AP UT WOS:000237272100030 ER PT J AU Eckart, A Baganoff, FK Schodel, R Morris, M Genzel, R Bower, GC Marrone, D Moran, JM Viehmann, T Bautz, MW Brandt, WN Garmire, GP Ott, T Trippe, S Ricker, GR Straubmeier, C Roberts, DA Yusef-Zadeh, F Zhao, JH Rao, R AF Eckart, A Baganoff, FK Schodel, R Morris, M Genzel, R Bower, GC Marrone, D Moran, JM Viehmann, T Bautz, MW Brandt, WN Garmire, GP Ott, T Trippe, S Ricker, GR Straubmeier, C Roberts, DA Yusef-Zadeh, F Zhao, JH Rao, R TI The flare activity of Sagittarius A - New coordinated mm to X-ray observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; X-rays : general; infrared : general; accretion, accretion disks; Galaxy : center; Galaxy : nucleus ID SUPERMASSIVE BLACK-HOLE; DOMINATED ACCRETION FLOWS; GALACTIC-CENTER; SGR-A; LINEAR-POLARIZATION; STELLAR DYNAMICS; PROPER MOTIONS; RADIO-SOURCES; MILKY-WAY; ASTERISK AB Context. We report new simultaneous near-infrared/sub-millimeter/X-ray observations of the SgrA* counterpart associated with the massive 3-4 x 10(6) M-circle dot black hole at the Galactic Center. Aims. We investigate the physical processes responsible for the variable emission from SgrA*. Methods. The observations have been carried out using the NACO adaptive optics (AO) instrument at the European Southern Observatory's Very Large Telescope(star) and the ACIS-I instrument aboard the Chandra X-ray Observatory as well as the Submillimeter Array SMA(star star) on Mauna Kea, Hawaii, and the Very Large Array(star star star) in New Mexico. Results. We detected one moderately bright flare event in the X-ray domain and 5 events at infrared wavelengths. The X-ray flare had an excess 2-8 keV luminosity of about 33 x 10(33) erg/s. The duration of this flare was completely covered in the infrared and it was detected as a simultaneous NIR event with a time lag of <= 10 min. Simultaneous infrared/X-ray observations are available for 4 flares. All simultaneously covered flares, combined with the flare covered in 2003, indicate that the time-lag between the NIR and X-ray flare emission is very small and in agreement with a synchronous evolution. There are no simultaneous flare detections between the NIR/X-ray data and the VLA and SMA data. The excess flux densities detected in the radio and sub-millimeter domain may be linked with the flare activity observed at shorter wavelengths. Conclusions. We find that the flaring state can be explained with a synchrotron self-Compton (SSC) model involving up-scattered submillimeter photons from a compact source component. This model allows for NIR flux density contributions from both the synchrotron and SSC mechanisms. Indications for an exponential cutoff the NIR/MIR synchrotron spectrum allow for a straightforward explanation of the variable and red spectral indices of NIR flares. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. MIT, Space Res Ctr, Cambridge, MA 02139 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Eckart, A (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM eckart@ph1.uni-koeln.de; fkb@space.mit.edu; morris@astro.ucla.edu; gbower@astro.berkeley.edu RI Schoedel, Rainer/D-4751-2014; Brandt, William/N-2844-2015; OI Schoedel, Rainer/0000-0001-5404-797X; Brandt, William/0000-0002-0167-2453; Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 NR 85 TC 131 Z9 132 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 MAY PY 2006 VL 450 IS 2 BP 535 EP 555 DI 10.1051/0004-6361:20054418 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031LZ UT WOS:000236707400010 ER PT J AU Wu, Y Zhang, Q Yu, W Miller, M Mao, R Sun, K Wang, Y AF Wu, Y Zhang, Q Yu, W Miller, M Mao, R Sun, K Wang, Y TI Ammonia cores in high mass star formation regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE masers; ISM : clouds; ISM : kinematics and dynamics; stars : formation ID ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; NRAO PMN SURVEYS; H-II REGIONS; MOLECULAR CLOUDS; DARK CLOUDS; DENSE CORES; PROTOSTELLAR CANDIDATES; PHYSICAL-PROPERTIES; ARCETRI CATALOG AB We observed a sample of 35 water masers not coincident with known HII regions and/or low mass young stellar objects (YSOs) with the Effelsberg 100 m telescope in the NH3(J,K) = (1,1), (2,2), (3,3) and (4,4) transitions. Sixteen sources were detected in the NH3 emission. The detection rate is 46%. All these sixteen sources have NH3 (1,1) and (2,2) emission, among which four sources have NH3 (3,3) emission. Comparing with the IRAS and the 2MASS data, we analyzed the relationship between the detection rate and the infrared color, the dust temperature and the source distance. All the detected sources were mapped and 17 cores were obtained (one source IRAS 20215+3725 has two cores). From the detected sources five cores do not coincide with radio continuum or IRAS and MSX point sources. Excluding one core that has no MSX data available, the remaining eleven cores are coincident with IRAS or MSX point sources. The typical size and mass of the cores are 1.6 pc and 1.5 x 10(3) M-circle dot, respectively. The average line widths of the NH3 (1,1) and (2,2) are 1.54 and 1.73 km s(-1). The average kinetic temperature of the gas is about 19 K. These values are much larger than those of low mass cores. The NH3 cores that coincide with IRAS sources (referred to as Group I) have slightly larger line widths (1.65 and 1.75 km s(-1) for the (1,1) and (2,2) lines, respectively) and larger masses (1.8 x 10(3) M-circle dot) than the mean values of the sample. For this type of core the kinetic temperature correlates with the line width. The line width appears to correlate with the bolometric luminosity and the core size. Despite the average luminosity of 2.9 x 10(4) L-circle dot, there is no detectable 6 cm emission. These are candidates for high mass protostars or precursors of UC HII regions. The NH3 cores with peaks onset from infrared sources (referred to as Group II) have an average size of 1.7 pc and an average line width of 1.50 km s(-1) for the (1,1) line. The line width of the (1,1) emission is smaller than that of the group I. The average mass is 9.4 x 10(2) M-circle dot. One possible explanation for the deviation is that the NH3 peak and the infrared source correspond to different clumps. These cores are potential high mass star formation sites and may be at an earlier evolutionary stage than those with IRAS point sources. This type of core is seen in mapping observations, and can be easily missed by single-spectrum observations toward the IRAS position. C1 Peking Univ, Dept Astron, CAS, PKU Joint Beijing Astrophys Ctr, Beijing 100871, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bonn, Inst Inorgan Chem, D-53117 Bonn, Germany. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Wu, Y (reprint author), Peking Univ, Dept Astron, CAS, PKU Joint Beijing Astrophys Ctr, Beijing 100871, Peoples R China. EM yfwu@bac.pku.edu.cn OI Zhang, Qizhou/0000-0003-2384-6589 NR 48 TC 32 Z9 32 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 MAY PY 2006 VL 450 IS 2 BP 607 EP NL_30 DI 10.1051/0004-6361:20053203 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 031LZ UT WOS:000236707400015 ER PT J AU Zhang, JS Henkel, C Kadler, M Greenhill, LJ Nagar, N Wilson, AS Braatz, JA AF Zhang, JS Henkel, C Kadler, M Greenhill, LJ Nagar, N Wilson, AS Braatz, JA TI Extragalactic H2O masers and X-ray absorbing column densities SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE masers; galaxies : active; galaxies : nuclei; galaxies : statistics; radio lines : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; XMM-NEWTON OBSERVATION; HUBBLE-SPACE-TELESCOPE; ASCA OBSERVATIONS; WATER-VAPOR; BLACK-HOLE; BEPPOSAX OBSERVATIONS; CHANDRA OBSERVATIONS AB Having conducted a search for the lambda similar to 1.3 cm (22 GHz) water vapor line towards galaxies with nuclear activity, large nuclear column densities or high infrared luminosities, we present H2O spectra for NGC2273, UGC 5101, and NGC 3393 with isotropic luminosities of 7, 1500, and 400 L circle dot. The H2O maser in UGC 5101 is by far the most luminous yet found in an ultraluminous infrared galaxy. NGC 3393 reveals the classic spectrum of a "disk maser", represented by three distinct groups of Doppler components. As in all other known cases except NGC 4258, the rotation velocity of the putative masing disk is well below 1000 km s(-1). Based on the literature and archive data, X-ray absorbing column densities are compiled for the 64 galaxies with reported maser sources beyond the Magellanic Clouds. For NGC 2782 and NGC 5728, we present Chandra archive data that indicate the presence of an active galactic nucleus in both galaxies. Modeling the hard nuclear X-ray emission, NGC 2782 is best fit by a high energy reflection spectrum with N-H greater than or similar to 1024 cm(-2). For NGC 5728, partial absorption with a power law spectrum indicates N-H similar to 8 x 10(23) cm(-2). The correlation between absorbing column and H2O emission is analyzed. There is a striking difference between kilo- and megamasers with megamasers being associated with higher column densities. All kilomasers ( L-H2O < 10 L circle dot) except NGC 2273 and NGC 5194 are Compton-thin, i.e. their absorbing columns are < 10(24) cm(-2). Among the H2O megamasers, 50% arise from Compton-thick and 85% from heavily obscured (> 10(23) cm(-2)) active galactic nuclei. These values are not larger but consistent with those from samples of Seyfert 2 galaxies not selected on the basis of maser emission. The similarity in column densities can be explained by small deviations in position between maser spots and nuclear X-ray source and a high degree of clumpiness in the circumnuclear interstellar medium. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Guangzhou Univ, Ctr Astrophys, Guangzhou 510400, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Concepcion, Astron Grp, Concepcion, Chile. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM jzhang@mpifr-bonn.mpg.de OI Kadler, Matthias/0000-0001-5606-6154 NR 142 TC 54 Z9 57 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2006 VL 450 IS 3 BP 933 EP U16 DI 10.1051/0004-6361:20054138 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032TK UT WOS:000236797400008 ER PT J AU Clocchiatti, A Schmidt, BP Filippenko, AV Challis, P Coil, AL Covarrubias, R Diercks, A Garnavich, P Germany, L Gilliland, R Hogan, C Jha, S Kirshner, RP Leibundgut, B Leonard, D Li, WD Matheson, T Phillips, MM Prieto, JL Reiss, D Riess, AG Schommer, R Smith, RC Soderberg, A Spyromilio, J Stubbs, C Suntzeff, NB Tonry, JL Woudt, P AF Clocchiatti, A Schmidt, BP Filippenko, AV Challis, P Coil, AL Covarrubias, R Diercks, A Garnavich, P Germany, L Gilliland, R Hogan, C Jha, S Kirshner, RP Leibundgut, B Leonard, D Li, WD Matheson, T Phillips, MM Prieto, JL Reiss, D Riess, AG Schommer, R Smith, RC Soderberg, A Spyromilio, J Stubbs, C Suntzeff, NB Tonry, JL Woudt, P TI Hubble Space Telescope and ground-based observations of Type Ia supernovae at redshift 0.5: Cosmological implications SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; distance scale; galaxies : distances and redshifts; supernovae : general ID ACCELERATING UNIVERSE; LIGHT CURVES; DARK ENERGY; DECELERATION; CONSTRAINTS; CALIBRATION; PARAMETERS; PHOTOMETRY; CONSTANT; LAMBDA AB We present observations of the Type Ia supernovae (SNe) 1999M, 1999N, 1999Q, 1999S, and 1999U, at redshift z approximate to 0.5. They were discovered in early 1999 with the 4.0m Blanco telescope at Cerro Tololo Inter-American Observatory by the High-z Supernova Search Team(HZT) and subsequently followed with many ground-based telescopes. SNe 1999Q and 1999U were also observed with the Hubble Space Telescope. We computed luminosity distances to the new SNe using two methods and added them to the high-z Hubble diagram that the HZT has been constructing since 1995. The new distance moduli confirm the results of previous work. At z approximate to 0: 5, luminosity distances are larger than those expected for an empty universe, implying that a "cosmological constant,'' or another form of "dark energy,'' has been increasing the expansion rate of the universe during the last few billion years. Combining these new HZT SNe Ia with our previous results and assuming a Delta CDM cosmology, we estimate the cosmological parameters that best fit our measurements. For a sample of 75 low-redshift and 47 high-redshift SNe Ia with MLCS2k2 (Jha and coworkers) luminosity calibration we obtain Omega(M) = 0: 79(-0.18)(+0.15) and Omega(Lambda) = 1.57(-0.32)(+0.24) (1 sigma uncertainties) if no constraints are imposed, or Omega(M) = 0.29(-0.05)(+0.06) if Omega(M) + Omega(Lambda) = 1 is assumed. For a different sample of 58 low-redshift and 48 high-redshift SNe Ia with luminosity calibrations done using the PRES method (a generalization of the Delta m(15) method), the results are Omega(M) = 0.43(-0.19)(+0.17) and Omega(Lambda) = 1.18(-0.28)(+0.27) (1 sigma uncertainties) if no constraints are imposed, or Omega(M) = 0.18(-0.04)(+0.05) if Omega(M) + Omega(Lambda) = 1 is assumed. C1 Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Las Campanas Observ, La Serena, Chile. Cerro Tololo Interamer Observ, La Serena, Chile. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Clocchiatti, A (reprint author), Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Casilla 306, Santiago 22, Chile. EM aclocchi@astro.puc.cl; brian@mso.anu.edu.au; alex@astro.berkeley.edu; pchallis@cfa.harvard.edu; acoil@astro.berkeley.edu; pgarnavi@nd.edu; rgillila@stsci.edu; hogan@astro.washington.edu; sjha@astro.berkeley.edu; kirshner@cfa.harvard.edu; bleibund@eso.org; leonard@astro.caltech.edu; weidong@astro.berkeley.edu; matheson@noao.edu; prieto@astronomy.ohiostate.state.du; ariess@stsci.edu; csmith@ctio.noao.edu; jspyromi@eso.org; cstubbs@fas.harvard.edu; nsuntzeff@noao.edu; jt@ifa.hawaii.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 65 TC 96 Z9 99 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 MAY 1 PY 2006 VL 642 IS 1 BP 1 EP 21 DI 10.1086/498491 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600001 ER PT J AU Yoo, J Kochanek, CS Falco, EE McLeod, BA AF Yoo, J Kochanek, CS Falco, EE McLeod, BA TI Halo structures of gravitational lens galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dark matter; gravitational lensing; quasars : individual (B1938+666, HE 0435-1223, PG 1115+080, SDSS J0924+0219) ID DARK-MATTER SUBSTRUCTURE; DIGITAL SKY SURVEY; OCCUPATION DISTRIBUTION; PG 1115+080; GALACTIC SATELLITES; SUBHALO POPULATIONS; FIELD GALAXIES; MG J0414+0534; FLUX RATIOS; TIME DELAYS AB We explore the halo structure of four gravitational lenses with well-observed, thin Einstein rings. We find that the gravitational potentials are well described by ellipsoidal density distributions in the sense that the best-fit non-ellipsoidal models have parameters consistent with their ellipsoidal counterparts. We find upper limits on the standard parameters for the deviation from an ellipse of vertical bar a(3)(B)/a(0)vertical bar < 0.023, 0.019, 0.037, and 0.035 and vertical bar a(4)(B)/a(0)vertical bar < 0.034, 0.041, 0.051, and 0.064 for SDSS J0924+0219, HE 0435-1223, B1938+666, and PG 1115+080, respectively. We find that the lens galaxies are at the centers of their dark matter halos and obtain upper limits for the offset of each center of mass from the center of light of vertical bar Delta x vertical bar < 0."004, 0."005, 0."009, and 0."005, corresponding to 22, 29, 70, and 23 pc, respectively. These limits also exclude the possibility of any significant lopsidedness of the dark matter halos and set an upper limit of fsat less than or similar to root N% on the mass fraction of massive substructures inside the Einstein ring if they are divided over N satellites. We also explore the properties of galaxies as substructures in groups for the lens PG 1115+080, finding evidence for dark matter halos associated with the galaxies but no evidence for a clear distinction between satellite and central galaxies. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoo, J (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM jaiyul@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu; efalco@cfa.harvard.edu; bmcleod@cfa.harvard.edu NR 63 TC 31 Z9 31 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2006 VL 642 IS 1 BP 22 EP 29 DI 10.1086/500968 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600002 ER PT J AU Evans, DA Worrall, DM Hardcastle, MJ Kraft, RP Birkinshaw, M AF Evans, DA Worrall, DM Hardcastle, MJ Kraft, RP Birkinshaw, M TI Chandra and Xmm-Newton observations of a sample of low-redshift FR I and FR II radio galaxy nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : jets; X-rays : galaxies ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; UNIFIED SCHEMES; CENTAURUS-A; CYGNUS-A; 3C 390.3; ENERGY-DISTRIBUTIONS; IONIZED-GAS AB We present spectral results from Chandra and XMM-Newton observations of a sample of 22 low-redshift (z < 0.1) radio galaxies and consider whether the core emission originates from the base of a relativistic jet, or an accretion flow, or contains contributions from both. We find correlations between the unabsorbed X-ray, radio, and optical fluxes and luminosities of FR I-type radio-galaxy cores, implying a common origin in the form of a jet. On the other hand, we find that the X-ray spectra of FR II-type radio galaxy cores are dominated by absorbed emission, with NH greater than or similar to 10(23) atoms cm(-2), which is likely to originate in an accretion flow. We discuss several models that may account for the different nuclear properties of FR I- and FR II-type cores and also demonstrate that both heavily obscured, accretion-related and unobscured, jet-related components may be present in all radio galaxy nuclei. Any absorbed, accretion-related components in FR I- type galaxies have low radiative efficiencies. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RP Evans, DA (reprint author), Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 74 TC 130 Z9 130 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2006 VL 642 IS 1 BP 96 EP 112 DI 10.1086/500658 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600009 ER PT J AU Barmby, P Alonso-Herrero, A Donley, JL Egami, E Fazio, GG Georgakakis, A Huang, JS Laird, ES Miyazaki, S Nandra, K Park, SQ Perez-Gonzalez, PG Rieke, GH Rigby, JR Willner, SP AF Barmby, P Alonso-Herrero, A Donley, JL Egami, E Fazio, GG Georgakakis, A Huang, JS Laird, ES Miyazaki, S Nandra, K Park, SQ Perez-Gonzalez, PG Rieke, GH Rigby, JR Willner, SP TI Mid-infrared properties of X-ray sources in the extended groth strip SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; infrared : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; FRANCE REDSHIFT SURVEY; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; SPECTRAL ENERGY-DISTRIBUTIONS; DEEP SUBMILLIMETER SURVEY; LYMAN BREAK GALAXIES; STAR-FORMATION RATE; FIELD NORTH SURVEY; XMM-NEWTON SURVEYS AB Mid-infrared observations of active galactic nuclei (AGNs) are important for understanding the physical conditions around the central accretion engines. Chandra and XMM-Newton X-ray observations of a 300 arcmin(2) region in the extended Groth strip are used to select a sample of similar to 150 AGNs. The Spitzer instruments IRAC and MIPS detect 68%-80% of these sources, which show a wide range of mid-infrared properties. About 40% of the sources have red power-law spectral energy distributions (f(nu) proportional to nu(alpha), alpha similar to 0) in the 3.6 - 8 mu m IRAC bands. In these sources the central engine dominates the emission at both X-ray and IR wavelengths. Another 40% of the sources have blue mid-IR spectral energy distributions (alpha > 0) with their infrared emission dominated by the host galaxy; the remaining 20% are not well fit by a power law. Published IRAC color criteria for AGNs select most of the red sources, but only some of the blue sources. As with all other known methods, selecting AGNs with mid-IR colors will not produce a sample that is simultaneously complete and reliable. The IRAC SED type does not directly correspond to X-ray spectral type (hard/soft). The mid-IR properties of X-ray-detected Lyman break, radio, submillimeter, and optically faint sources vary widely, and for the most part are not distinct from those of the general X-ray/infrared source population. X-ray sources emit 6%-11% of the integrated mid-IR light, making them significant contributors to the cosmic infrared background. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, Dept Astrofis Mol & Infrarroja, Inst Estructura Mat, E-28006 Madrid, Spain. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Imperial Coll London, Astrophys Grp, Blackett Lab, London SW7 2AW, England. Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 65, Cambridge, MA 02138 USA. RI Georgakakis, Antonis/K-4457-2013; Rigby, Jane/D-4588-2012; Barmby, Pauline/I-7194-2016; Perez-Gonzalez, Pablo/J-2871-2016; Alonso-Herrero, Almudena/H-1426-2015; OI Rigby, Jane/0000-0002-7627-6551; Barmby, Pauline/0000-0003-2767-0090; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Alonso-Herrero, Almudena/0000-0001-6794-2519; Georgakakis, Antonis/0000-0002-3514-2442 NR 67 TC 89 Z9 89 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 MAY 1 PY 2006 VL 642 IS 1 BP 126 EP 139 DI 10.1086/500823 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600011 ER PT J AU Sasaki, M Gaetz, TJ Blair, WP Edgar, RJ Morse, JA Plucinsky, PP Smith, RK AF Sasaki, M Gaetz, TJ Blair, WP Edgar, RJ Morse, JA Plucinsky, PP Smith, RK TI Far-Ultraviolet and X-ray observations of the reverse shock in the Small Magellanic Cloud supernova remnant 1E 0102.2-7219 SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; supernova remnants; ultraviolet : ISM; X-rays : individual (1E 0102.2-7219) ID MOLECULAR-HYDROGEN; EXTINCTION CURVES; YOUNG; 1E-0102.2-7219; ABUNDANCES; SPECTRUM; INSTABILITIES; ELEMENTS; ATLAS AB We present Far Ultraviolet Spectroscopic Explorer (FUSE) and X-Ray Multi-Mirror Mission (XMM-Newton) data for the reverse shock of the O-rich supernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud (SMC). The FUSE observations cover three regions with significantly different optical [O (III)] intensities, all associated with the relatively bright part of the X-ray ring. Emission lines of O (VI) lambda lambda 1032, 1038 are clearly detected in the FUSE spectra. The XMM-Newton EPIC MOS 1/2 spectra are dominated by strong emission lines of O, Ne, and Mg. By combining the O (VI) doublet emission with the O (VII) triplet and O (VIII) Ly alpha fluxes from the X-ray spectra and assuming a nonequilibrium ionization (NEI) model with a single ionization timescale for the spectra, we find an increase of the ionization timescale tau from north (tau approximate to 0.6 x 10(11) s cm(-3)) to southeast (tau approximate to 2 x 10(11) s cm(-3)). This is indicative of increasing density in the X-ray-bright ring, in good agreement with the optical [O (III)] emission, which is strongest in the southeast. However, if we assume a plane-parallel shock model with a distribution of ionization timescales, the O (VI) emission appears to be inconsistent with O (VII) and O (VIII) in X-rays. The analysis of the total X-ray spectra shows that there is no consistent set of values for the temperature and ionization timescale that can explain the observed line ratios for O, Ne, and Mg. This would be consistent with a structured distribution of the ejecta, as the O, Ne, and Mg would have interacted with the reverse shock at different times. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msasaki@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016 OI Sasaki, Manami/0000-0001-5302-1866 NR 35 TC 11 Z9 11 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2006 VL 642 IS 1 BP 260 EP 269 DI 10.1086/500789 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600021 ER PT J AU Cooper, RL Mukhopadhyay, B Steeghs, D Narayan, R AF Cooper, RL Mukhopadhyay, B Steeghs, D Narayan, R TI On the production and survival of carbon fuel for superbursts on accreting neutron stars: Implications for mass donor evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE dense matter; nuclear reactions, nucleosynthesis, abundances; stars : neutron; X-rays : binaries; X-rays : bursts ID X-RAY-BURSTS; WEAK-INTERACTION RATES; THERMONUCLEAR REACTION-RATES; XMM-NEWTON OBSERVATIONS; GX 17+2; CATACLYSMIC VARIABLES; BLACK-HOLES; RP-PROCESS; 4U 1636-53; NUCLEOSYNTHESIS AB We have investigated the physical conditions under which accreting neutron stars in low-mass X-ray binaries can both produce and preserve sufficient quantities of carbon fuel to trigger superbursts. Our theoretical models span the plausible ranges of neutron star thermal conductivities, core neutrino emission mechanisms, and areal radii, as well as the CNO abundances in the accreted material. We find that neutron stars that accrete hydrogen-rich material with CNO mass fractions Z(CNO) less than or similar to Z(CNO,circle dot) will not exhibit superbursts under any circumstances. Neutron stars that accrete material with CNO mass fractions greater than or similar to 4Z(CNO,circle dot) will exhibit superbursts at accretion rates in the observed range. On this basis, we suggest that the mass donors of superburst systems must have enhanced CNO abundances. The accreted CNO acts only as a catalyst for hydrogen burning via the hot CNO cycle, and therefore it is the sum of the three elements' mass fractions, not the individual mass fractions themselves, that is important. Systems that exhibit superbursts are observed to differ from those that do not exhibit superbursts in the nature of their helium-triggered type I X-ray bursts: the bursts have shorter durations and much greater alpha-values. Increasing the CNO abundance of the accreted material in our models reproduces both of these observations, thus once again suggesting enhanced CNO abundances in the mass donors. Many compact binary systems have been observed in which the abundances of the accreting material are distinctly nonsolar. Although abundance analyses of the systems that exhibit superbursts currently do not exist, Bowen fluorescence blend profiles of 4U 1636-536 and Ser X-1 suggest that the mass donor stars may indeed have nonsolar CNO metallicities. More detailed abundance analyses of the accreting matter in systems that exhibit superbursts are needed to verify our assertion that the matter is rich in CNO elements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cooper, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rcooper@cfa.harvard.edu; bmukhopa@cfa.harvard.edu; dsteeghs@cfa.harvard.edu; rnarayan@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Narayan, Ramesh/0000-0002-1919-2730 NR 89 TC 15 Z9 15 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 MAY 1 PY 2006 VL 642 IS 1 BP 443 EP 454 DI 10.1086/500922 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600037 ER PT J AU Aerts, C Marchenko, SV Matthews, JM Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH Weiss, WW AF Aerts, C Marchenko, SV Matthews, JM Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH Weiss, WW TI delta Ceti is not monoperiodic: Seismic modeling of a beta Cephei star from Most(1) space-based photometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : early-type; stars : individual (HD 16582); stars : oscillations; stars : variables : other ID PULSATIONAL FREQUENCY-ANALYSIS; NU-ERIDANI; THETA-OPHIUCHI; SCUTI STAR; ASTEROSEISMOLOGY; IDENTIFICATION; STANDARD AB The beta Cephei star delta Ceti was considered one of the few monoperiodic variables in its class. Despite ( or perhaps because of) its apparently simple oscillation spectrum, it has been challenging and controversial to identify this star's pulsation mode and constrain its physical parameters seismically. Broadband time-resolved photometry of delta Ceti spanning 18.7 days with a duty cycle of about 65% obtained by the Microvariability and Oscillations of Stars ( MOST) satellite-the first scientific observations ever obtained by MOST-reveals that the star is actually multiperiodic. Besides the well-known dominant frequency of f(1) = 6.205886 day(-1), we have discovered in the MOST data its first harmonic 2f(1) and three other frequencies (f(2) 3.737, f(3) 3.673, and f(4) = 0.318 day(-1)), all detected with a signal-to-noise ratio (S/N) > 4. In retrospect, f(2) was also present in archival spectral line-profile data but at lower S/N. We present seismic models whose modes match exactly the frequencies f1 and f2. Only one model falls within the common part of the error boxes of the star's observed surface gravity and effective temperature from photometry and spectroscopy. In this model, f1 is the radial (l = 0) first overtone, and f(2) is the g(2) (l = 2, m = 0) mode. This model has a mass of 10.2 +/- 0.2 M-circle dot and an age of 17.9 +/- 0: 3 Myr, making delta Ceti an evolved beta Cephei star. If f(2) and f(3) are rotationally split components of the same g2 mode, then the star's equatorial rotation velocity is either 27.6 km s(-1) or half this value. Given its v sin i of about 1 km s(-1), this implies that we are seeing delta Ceti nearly pole-on. C1 Katholieke Univ Leuven, Inst Astron, B-3001 Heverlee, Belgium. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Aerts, C (reprint author), Katholieke Univ Leuven, Inst Astron, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium. EM conny@ster.kuleuven.be NR 32 TC 34 Z9 34 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2006 VL 642 IS 1 BP 470 EP 477 DI 10.1086/500800 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038GH UT WOS:000237206600040 ER PT J AU Fish, VL Reid, MJ AF Fish, VL Reid, MJ TI Full-polarization observations of OH masers in massive star-forming regions. II. Maser properties and the interpretation of polarization SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE ISM : molecules; magnetic fields; masers; polarization; radio lines : ISM; stars : formation ID YOUNG STELLAR OBJECTS; RECOMBINATION LINE OBSERVATIONS; INTERSTELLAR HYDROXYL MASERS; SINGULAR ISOTHERMAL TOROIDS; MAGNETIC-FIELD STRUCTURE; NGC-7538 IRS-1 REGION; GHZ METHANOL MASERS; CEPHEUS-A; HII-REGIONS; EXCITED OH AB We analyze full-polarization VLBA data of ground-state OH masers in 18 massive star-forming regions previously presented in a companion paper. We confirm results previously seen in the few individual sources studied at milliarcsecond angular resolution. The OH masers often arise in the shocked neutral gas surrounding ultracompact H II regions. Magnetic fields as deduced from OH maser Zeeman splitting are highly ordered on the scale of a source and on the maser clustering scale of similar to 10(15) cm, which appears to be universal. OH masers around ultracompact H II regions live similar to 10(4) yr before turning off abruptly, rather than weakening gradually. These masers have a wide range of polarization properties. At one extreme (e.g., W75 N), pi-components are detected and the polarization position angles of maser spots show some organization. At the other extreme (e.g., W51 e1/e2), almost no linear polarization is detected and partial depolarization occurs. A typical source has properties intermediate to these two extremes, with no clear pattern in the distribution of polarization position angles. This can be explained if Faraday rotation in a typical OH maser source is large on a maser amplification length but small on a single (e-folding) gain length. Increasing or decreasing Faraday rotation by a factor of similar to 5 among different sources can explain the observed variation in polarization properties. Pure pi-components (in theory, 100% linearly polarized) are seldom seen. We suggest that almost all pi-components acquire a significant amount of circular polarization from low-gain stimulated emission of a sigma-component from velocity-coherent OH lying along the propagation path. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Fish, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vfish@nrao.edu; reid@cfa.harvard.edu NR 147 TC 44 Z9 44 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2006 VL 164 IS 1 BP 99 EP 123 DI 10.1086/502650 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039JD UT WOS:000237300900005 ER PT J AU Wright, SJ Muller-Landau, HC AF Wright, SJ Muller-Landau, HC TI The future of tropical forest species SO BIOTROPICA LA English DT Review DE Brazil; conservation; deforestation; extinction; habitat loss; human population growth; secondary forest; tropical biodiversity ID RAIN-FOREST; AMAZONIAN FORESTS; DEFORESTATION; BIODIVERSITY; CARBON; COMMUNITIES; EXTINCTIONS; REGROWTH; RECOVERY; HOTSPOTS AB Deforestation and habitat loss are widely expected to precipitate an extinction crisis among tropical forest species. Humans cause deforestation, and humans living in rural settings have the greatest impact on extant forest area in the tropics. Current human demographic trends, including slowing population growth and intense urbanization, give reason to hope that deforestation will slow, natural forest regeneration through secondary succession will accelerate, and the widely anticipated mass extinction of tropical forest species will be avoided. Here, we show that the proportion of potential forest cover remaining is closely correlated with human population density among countries, in both the tropics and the temperate zone. We use United Nations population projections and continent-specific relationships between both total and rural population density and forest remaining today to project future tropical forest cover. Our projections suggest that deforestation rates will decrease as population growth slows, and that a much larger area will continue to be forested than previous studies suggest. Tropical forests retracted to smaller areas during repeated Pleistocene glacial events in Africa and more recently in selected areas that supported large prehistoric human populations. Despite many caveats, these projections and observations provide hope that many tropical forest species will be able to survive the current wave of deforestation and human population growth. A strategy to preserve tropical biodiversity might include policies to improve conditions in tropical urban settings to hasten urbanization and preemptive conservation efforts in countries with large areas of extant forest and large projected rates of future human population growth. We hope that this first attempt inspires others to produce better models of future tropical forest cover and associated policy recommendations. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 57 TC 240 Z9 253 U1 23 U2 168 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2006 VL 38 IS 3 BP 287 EP 301 DI 10.1111/j.1744-7429.2006.00154.x PG 15 WC Ecology SC Environmental Sciences & Ecology GA 032HW UT WOS:000236766500001 ER PT J AU Piou, C Feller, IC Berger, U Chi, F AF Piou, C Feller, IC Berger, U Chi, F TI Zonation patterns of Belizean offshore mangrove forests 41 years after a catastrophic hurricane SO BIOTROPICA LA English DT Article DE Avicennia germinans; Belize; hurricane disturbances; Laguncularia racemosa; long-term regeneration; mangrove forest dynamics; Rhizophora mangle; species dominance heterogeneity; Turneffe Atoll; zonation patterns ID SPECIES DISTRIBUTION; NUTRIENT ENRICHMENT; FLORIDA; GROWTH; REGENERATION; RECRUITMENT; LIMITATION; PREDATION; DOMINANCE; DYNAMICS AB Mangroves are prone to bearing frequently the full brunt of hurricanes and tropical storms. The extent of destruction and early regeneration are widely studied. The purpose of this study was to add a long-term view of mangrove regeneration and assess the potential effects on mangrove horizontal zonation patterns of catastrophic destruction. Hattie, a category five hurricane, hit the Belizean coast in 1961. It passed directly over the Turneffe Atoll where our study area, Calabash Cay, is located. At four sites on this island, we analyzed mangrove forest structure along transects parallel to the shoreline within zones delineated by species dominance and tree height. We propose an index based on the Simpson index of diversity to express changes in the heterogeneity of the species dominance. Physical-chemical parameters and nutrient availability were also measured. The destruction levels were estimated by analysis of the distribution of diameter at breast heights of the bigger trees in the inland zones. Variations in species dominance among sites and zones could be explained by interactions of various factors. Further, different levels of destruction between the two sides of the island had a significant effect on current patterns of species and structural zonation at Calabash. We conclude that disturbance regime in general should be considered as a factor potentially influencing mangrove horizontal zonation patterns. C1 Ctr Trop Marine Ecol, D-23859 Bremen, Germany. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Belize, Inst Marine Studies, Belize City, Belize. RP Ctr Trop Marine Ecol, Fahrenheitstr 6, D-23859 Bremen, Germany. EM cyril.piou@zmt-bremen.de OI Feller, Ilka/0000-0002-6391-1608 NR 35 TC 33 Z9 38 U1 2 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD MAY PY 2006 VL 38 IS 3 BP 365 EP 374 DI 10.1111/j.1744-7429.2006.00156.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 032HW UT WOS:000236766500011 ER PT J AU Kalko, EKV Ueberschaer, K Dechmann, D AF Kalko, EKV Ueberschaer, K Dechmann, D TI Roost structure, modification, and availability in the white-throated round-eared bat, Lophostoma silvicolum (Phyllostomidae) living in active termite nests SO BIOTROPICA LA English DT Article DE Barro Colorado Island; Chiroptera; Lophostoma; Phyllostomidae; roost availability; roost modification; roost structure; termites ID THYROPTERA-TRICOLOR; CENTRAL AMAZONIA; CHIROPTERA; BEHAVIOR; ECOLOGY; FOREST AB We studied roost structure, modification, and availability in Lophostoma silvicolum (Phyllostomidae), an insectivorous gleaning bat, on Barro Colorado Island (BCI), Panama. Collection of nest material beneath termitaria and infrared video filming indicated that males of L. silvicolum excavate and maintain cavities inside active termite nests. A binary logistic regression analysis showed that to be suitable as roosts, termite nests have to be larger than 30 cm in diameter and taller than 30 cm, well shaded, with few transecting branches, and freely accessible from below. Use of active termite nests as roosts may provide several benefits to L. silvicolum, including reduction of competition for roost sites with sympatric bat species, reduced parasite load and a suitable microclimate. A comparison of number of all termite nests in selected forest plots with number of termite nests that are potentially suited as bat roosts and number of termite nests that are actually used by bats suggests that L. silvicolum may not be roost-limited on BCI in spite of its highly specialized roost choice. C1 Univ Ulm, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. Univ Tubingen, D-72076 Tubingen, Germany. Univ Zurich, Inst Zool, CH-8057 Zurich, Switzerland. RP Kalko, EKV (reprint author), Univ Ulm, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM Elisabeth.Kalko@uni-ulm.de RI Dechmann, Dina/A-1827-2010 NR 32 TC 16 Z9 17 U1 1 U2 8 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2006 VL 38 IS 3 BP 398 EP 404 DI 10.1111/j.1744-7429.2006.00142.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 032HW UT WOS:000236766500015 ER PT J AU Littler, MM Littler, DS Lapointe, BE Barile, PJ AF Littler, MM Littler, DS Lapointe, BE Barile, PJ TI Toxic Cyanobacteria (blue-green algae) associated with groundwater conduits in the Bahamas SO CORAL REEFS LA English DT Editorial Material C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Harbor Branch Oceanog Inst Inc, Div Marine Sci, Ft Pierce, FL 34946 USA. RP Littler, MM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, POB 37012,MRC 166, Washington, DC 20013 USA. EM litterm@si.edu NR 3 TC 10 Z9 12 U1 1 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAY PY 2006 VL 25 IS 2 BP 186 EP 186 DI 10.1007/s00338-005-0010-8 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 039GA UT WOS:000237292800002 ER PT J AU Croquer, A Bastidas, C Lipscomp, D Rodriguez-Martinez, RE Jordan-Dahlgren, E Guzman, HM AF Croquer, A Bastidas, C Lipscomp, D Rodriguez-Martinez, RE Jordan-Dahlgren, E Guzman, HM TI First report of folliculinid ciliates affecting Caribbean scleractinian corals SO CORAL REEFS LA English DT Article DE ciliates; Caribbean corals; emergent syndromes; coral diseases ID DISEASE; REEFS; PATHOGENS; ECOLOGY; SPREAD; SEA AB This is the first report of a ciliate of the genus Halofolliculina infecting hard coral species of six families (Acroporidae, Agaricidae, Astrocoeniidae, Faviidae, Meandrinidae and Poritidae) and milleporids in the Caribbean. Surveys conducted during 2004-2005 in Venezuela, Panama and Mexico confirmed that this ciliate affects up to 25 scleractinian species. The prevalence of this ciliate at the coral community level was variable across sites, being most commonly found at Los Roques, Venezuela, and at Bocas del Toro, Panama (prevalence 0.2-2.5%), but rarely observed in the Mexican Caribbean. Ciliates were more prevalent within populations of acroporids (Acropora palmata, Acropora cervicornis and Acropora prolifera) in Los Roques. Recent observations also corroborate the presence of these ciliates in Curacao and Puerto Rico. Our observations indicate that ciliates affecting corals have a wider distribution than previously thought, and are no longer exclusively found in the Indo-Pacific and Red Sea. C1 Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Cancun 77500, Q Roo, Mexico. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Croquer, A (reprint author), Univ Simon Bolivar, Dept Biol Organismos, Caracas 1080A, Venezuela. EM croquer@telcel.net.ve OI Croquer, Aldo/0000-0001-8880-9338 NR 23 TC 24 Z9 24 U1 2 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAY PY 2006 VL 25 IS 2 BP 187 EP 191 DI 10.1007/s00338-005-0068-3 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 039GA UT WOS:000237292800003 ER PT J AU Becerro, MA Bonito, V Paul, VJ AF Becerro, MA Bonito, V Paul, VJ TI Effects of monsoon-driven wave action on coral reefs of Guam and implications for coral recruitment SO CORAL REEFS LA English DT Article DE community structure dynamics; coral recruitment; Crustose coralline algae; Cyanobacteria; Pacific Ocean reefs; storm effects ID GREAT-BARRIER-REEF; LONG-TERM; BENTHIC CYANOBACTERIA; SECONDARY METABOLITES; HERBIVORE EXCLUSION; NUTRIENT ENRICHMENT; COMMUNITY STRUCTURE; LYNGBYA-MAJUSCULA; MACROALGAL BLOOMS; LOCAL DYNAMICS AB Benthic cyanobacteria can respond rapidly to favorable environmental conditions, overgrow a variety of reef organisms, and dominate benthic marine communities; however, little is known about the dynamics and consequences of such cyanobacterial blooms in coral reef ecosystems. In this study, the benthic community was quantified at the time of coral spawnings in Guam to assess the substrate that coral larvae would encounter when attempting settlement. Transects at 9, 18, and 25-m depths were surveyed at two reef sites before and after heavy wave action driven by westerly monsoon winds. Communities differed significantly between sites and depths, but major changes in benthic community structure were associated with wave action driven by monsoon winds. A shift from cyanobacteria to crustose coralline algae (CCA) accounted for 44% of this change. Coral recruitment on Guam may be limited by substrate availability if cyanobacteria cover large areas of the reef at the time of settlement, and consequently recruitment may in part depend upon wave action from annual monsoon winds and tropical storms which remove cyanobacteria, thereby exposing underlying CCA and other substrate suitable for coral settlement. C1 CSIC, Ctr Adv Studies, CEAB, Blanes 17300, Girona, Spain. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Florida Museum Nat Hist, Dept Malacol, Gainesville, FL 32611 USA. RP Becerro, MA (reprint author), CSIC, Ctr Adv Studies, CEAB, Acc C St Francesc 14, Blanes 17300, Girona, Spain. EM mikel@ceab.csic.es RI Becerro, Mikel/A-5325-2008; OI Becerro, Mikel/0000-0002-6047-350X NR 65 TC 14 Z9 16 U1 4 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAY PY 2006 VL 25 IS 2 BP 193 EP 199 DI 10.1007/s00338-005-0080-7 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 039GA UT WOS:000237292800005 ER PT J AU Toscano, MA Macintyre, IG AF Toscano, MA Macintyre, IG TI Reply to Gischler E, Comment on Toscano and Macintyre (2005): corrected western Atlantic sea-level curve for the last 11,000 years based on calibrated C-14 dates from Acropora palmata framework and intertidal mangrove peat Coral Reefs 22 : 257-270 (2003), and their response in Coral Reefs 24 : 187-190 (2005) SO CORAL REEFS LA English DT Editorial Material DE sea-level; Mangrove peat; Acropora palmata; storm rubble; reef stratigraphy; tectonics ID RECENT SEDIMENTARY RECORD; GULF-OF-MEXICO; SOUTHWESTERN COAST; FLORIDA; RISE; MAINE; STRATIGRAPHY; SUBMERGENCE; EVOLUTION; HISTORY C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Toscano, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121,POB 37012, Washington, DC 20013 USA. EM toscanom@si.edu NR 38 TC 6 Z9 6 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAY PY 2006 VL 25 IS 2 BP 281 EP 286 DI 10.1007/s00338-006-0102-0 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 039GA UT WOS:000237292800022 ER PT J AU Gilbert, B Wright, SJ Muller-Landau, HC Kitajima, K Hernandez, A AF Gilbert, Benjamin Wright, S. Joseph Muller-Landau, Helene C. Kitajima, Kaoru Hernandez, Andres TI Life history trade-offs in tropical trees and lianas SO ECOLOGY LA English DT Article DE growth; liana; life history; ontogenetic shift; sapling; seedling; shade tolerance; survival; trade-offs; tropical forest ID NEOTROPICAL RAIN-FOREST; RELATIVE IMPORTANCE; SPECIES-DIVERSITY; GROWTH; SHADE; RECRUITMENT; PATTERNS; CANOPY; HEIGHT; MODELS AB It has been hypothesized that tropical trees partition forest light environments through a life history trade-off between juvenile growth and survival; however, the generality of this trade-off across life stages and functional groups has been questioned. We quantified trade-offs between growth and survival for trees and lianas on Barro Colorado Island (BCI), Panama using first-year seedlings of 22 liana and 31 tree species and saplings (10 mm < dbh < 39 mm) of 30 tree species. Lianas showed trade-offs similar to those of trees, with both groups exhibiting broadly overlapping ranges in survival and relative growth rates as seedlings. Life history strategies at,the seedling stage were highly correlated with those at the sapling stage among tree species, with all species showing an increase in survival with size. Only one of 30 tree species demonstrated a statistically significant ontogenetic shift, having a relatively lower Survival rate at the sapling stage than expected. Our results indicate that similar life history trade-offs apply across two functional groups (lianas and trees), and that life history strategies are largely conserved across seedling and sapling life-stages for most tropical tree species. C1 Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Minnesota, St Paul, MN 55108 USA. Univ Florida, Gainesville, FL 32611 USA. RP Gilbert, B (reprint author), Univ British Columbia, Dept Bot, Room 3529,6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM bgilbert@zoology.ubc.ca RI Gilbert, Benjamin/E-6616-2010; Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Gilbert, Benjamin/0000-0002-4947-6822; Wright, Stuart/0000-0003-4260-5676 NR 47 TC 78 Z9 84 U1 5 U2 35 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 MAY PY 2006 VL 87 IS 5 BP 1281 EP 1288 DI 10.1890/0012-9658(2006)87[1281:LHTITT]2.0.CO;2 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 042TM UT WOS:000237552400023 PM 16761606 ER PT J AU Hardesty, BD Hubbell, SP Bermingham, E AF Hardesty, BD Hubbell, SP Bermingham, E TI Genetic evidence of frequent long-distance recruitment in a vertebrate-dispersed tree SO ECOLOGY LETTERS LA English DT Article DE Barro Colorado Island; frugivory; microsatellites; Panama; parentage analysis; pollen movement; seed dispersal; seedling establishment; Simarouba amara; tropical forest ID SEED DISPERSAL; TROPICAL FOREST; PATERNITY ANALYSIS; NEOTROPICAL TREE; POPULATION-GENETICS; SIMAROUBA-AMARA; RAIN-FOREST; PATTERNS; PLANTS; FLOW AB The importance of dispersal for the maintenance of biodiversity, while long-recognized, has remained unresolved. We used molecular markers to measure effective dispersal in a natural population of the vertebrate-dispersed Neotropical tree, Simarouba amara (Simaroubaceae) by comparing the distances between maternal parents and their offspring and comparing gene movement via seed and pollen in the 50 ha plot of the Barro Colorado Island forest, Central Panama. In all cases (parent-pair, mother-offspring, father-offspring, sib-sib) distances between related pairs were significantly greater than distances to nearest possible neighbours within each category. Long-distance seedling establishment was frequent: 74% of assigned seedlings established > 100 m from the maternal parent [mean = 392 +/- 234.6 m (SD), range = 9.3-1000.5 m] and pollen-mediated gene flow was comparable to that of seed [mean = 345.0 +/- 157.7 m (SD), range 57.6-739.7 m]. For S. amara we found approximately a 10-fold difference between distances estimated by inverse modelling and mean seedling recruitment distances (39 m vs. 392 m). Our findings have important implications for future studies in forest demography and regeneration, with most seedlings establishing at distances far exceeding those demonstrated by negative density-dependent effects. C1 Univ Reading, Sch Biol Sci, Reading RG6 6AS, Berks, England. Univ Georgia, Smithsonian Trop Res Inst, Athens, GA 30602 USA. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. RP Univ Reading, Sch Biol Sci, Reading RG6 6AS, Berks, England. EM b.d.hardesty@reading.ac.uk RI Hardesty, Britta Denise/A-3189-2011 OI Hardesty, Britta Denise/0000-0003-1948-5098 NR 57 TC 99 Z9 103 U1 0 U2 37 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2006 VL 9 IS 5 BP 516 EP 525 DI 10.1111/j.1461-0248.2006.00897.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 032UB UT WOS:000236799600002 PM 16643297 ER PT J AU Muller-Landau, HC Condit, RS Chave, J Thomas, SC Bohlman, SA Bunyavejchewin, S Davies, S Foster, R Gunatilleke, S Gunatilleke, N Harms, KE Hart, T Hubbell, SP Itoh, A Kassim, AR LaFrankie, JV Lee, HS Losos, E Makana Jr Ohkubo, T Sukumar, R Sun, IF Supardi, NMN Tan, S Thompson, J Valencia, R Munoz, GV Wills, C Yamakura, T Chuyong, G Dattaraja, HS Esufali, S Hall, P Hernandez, C Kenfack, D Kiratiprayoon, S Suresh, HS Thomas, D Vallejo, MI Ashton, P AF Muller-Landau, HC Condit, RS Chave, J Thomas, SC Bohlman, SA Bunyavejchewin, S Davies, S Foster, R Gunatilleke, S Gunatilleke, N Harms, KE Hart, T Hubbell, SP Itoh, A Kassim, AR LaFrankie, JV Lee, HS Losos, E Makana, JR Ohkubo, T Sukumar, R Sun, IF Supardi, NMN Tan, S Thompson, J Valencia, R Munoz, GV Wills, C Yamakura, T Chuyong, G Dattaraja, HS Esufali, S Hall, P Hernandez, C Kenfack, D Kiratiprayoon, S Suresh, HS Thomas, D Vallejo, MI Ashton, P TI Testing metabolic ecology theory for allometric scaling of tree size, growth and mortality in tropical forests SO ECOLOGY LETTERS LA English DT Article DE asymmetric competition; demographic rates; forest dynamics; light availability; metabolic theory of ecology; resource competition theory; tree allometry ID GENERAL-MODEL; NEOTROPICAL TREE; SHADE TOLERANCE; ADULT STATURE; LIGHT; ARCHITECTURE; DENSITY; PLANTS; HEIGHT; RATES AB The theory of metabolic ecology predicts specific relationships among tree stem diameter, biomass, height, growth and mortality. As demographic rates are important to estimates of carbon fluxes in forests, this theory might offer important insights into the global carbon budget, and deserves careful assessment. We assembled data from 10 old-growth tropical forests encompassing censuses of 367 ha and > 1.7 million trees to test the theory's predictions. We also developed a set of alternative predictions that retained some assumptions of metabolic ecology while also considering how availability of a key limiting resource, light, changes with tree size. Our results show that there are no universal scaling relationships of growth or mortality with size among trees in tropical forests. Observed patterns were consistent with our alternative model in the one site where we had the data necessary to evaluate it, and were inconsistent with the predictions of metabolic ecology in all forests. C1 Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Univ Toulouse 3, CNRS, UPS, Lab Evolut & Divers Biol,UMR 5174, F-31062 Toulouse, France. Univ Toronto, Fac Forestry, Toronto, ON, Canada. Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ USA. Res Off, Natl Pks Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. Field Museum, Chicago, IL 60605 USA. Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Wildlife Conservat Soc, Internatl Programs, Bronx, NY 10460 USA. RP Muller-Landau, HC (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA. EM hmuller@umn.edu RI Thomas, Sean/B-6089-2008; Thompson, Jill/K-2200-2012 OI Thompson, Jill/0000-0002-4370-2593 NR 53 TC 147 Z9 158 U1 9 U2 72 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 MAY PY 2006 VL 9 IS 5 BP 575 EP 588 DI 10.1111/j.1461-0248.2006.00904.x PG 14 WC Ecology SC Environmental Sciences & Ecology GA 032UB UT WOS:000236799600008 PM 16643303 ER PT J AU Muller-Landau, HC Condit, RS Harms, KE Marks, CO Thomas, SC Bunyavejchewin, S Chuyong, G Co, L Davies, S Foster, R Gunatilleke, S Gunatilleke, N Hart, T Hubbell, SP Itoh, A Kassim, AR Kenfack, D LaFrankie, JV Lagunzad, D Lee, HS Losos, E Makana, JR Ohkubo, T Samper, C Sukumar, R Sun, IF Supardi, NMN Tan, S Thomas, D Thompson, J Valencia, R Vallejo, MI Munoz, GV Yamakura, T Zimmerman, JK Dattaraja, HS Esufali, S Hall, P He, FL Hernandez, C Kiratiprayoon, S Suresh, HS Wills, C Ashton, P AF Muller-Landau, HC Condit, RS Harms, KE Marks, CO Thomas, SC Bunyavejchewin, S Chuyong, G Co, L Davies, S Foster, R Gunatilleke, S Gunatilleke, N Hart, T Hubbell, SP Itoh, A Kassim, AR Kenfack, D LaFrankie, JV Lagunzad, D Lee, HS Losos, E Makana, JR Ohkubo, T Samper, C Sukumar, R Sun, IF Supardi, NMN Tan, S Thomas, D Thompson, J Valencia, R Vallejo, MI Munoz, GV Yamakura, T Zimmerman, JK Dattaraja, HS Esufali, S Hall, P He, FL Hernandez, C Kiratiprayoon, S Suresh, HS Wills, C Ashton, P TI Comparing tropical forest tree size distributions with the predictions of metabolic ecology and equilibrium models SO ECOLOGY LETTERS LA English DT Article DE demographic rates; forest structure; large-scale disturbance; metabolic theory of ecology; old-growth forests; tree diameter distributions ID FREQUENCY-DISTRIBUTIONS; RAIN-FOREST; DIAMETER DISTRIBUTIONS; POPULATION-STRUCTURE; NORTHERN HARDWOODS; GENERAL-MODEL; DENSITY; DROUGHT; GROWTH; RECRUITMENT AB Tropical forests vary substantially in the densities of trees of different sizes and thus in above-ground biomass and carbon stores. However, these tree size distributions show fundamental similarities suggestive of underlying general principles. The theory of metabolic ecology predicts that tree abundances will scale as the -2 power of diameter. Demographic equilibrium theory explains tree abundances in terms of the scaling of growth and mortality. We use demographic equilibrium theory to derive analytic predictions for tree size distributions corresponding to different growth and mortality functions. We test both sets of predictions using data from 14 large-scale tropical forest plots encompassing censuses of 473 ha and > 2 million trees. The data are uniformly inconsistent with the predictions of metabolic ecology. In most forests, size distributions are much closer to the predictions of demographic equilibrium, and thus, intersite variation in size distributions is explained partly by intersite variation in growth and mortality. C1 Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Univ Toronto, Fac Forestry, Toronto, ON, Canada. Res Off, Natl Pks Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. Univ Buea, Dept Life Sci, Buea, Cameroon. Univ Philippines, Coll Sci, Inst Biol, Quezon City, Philippines. Field Museum, Chicago, IL 60605 USA. Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka. Wildlife Conservat Soc, Internatl Programs, Bronx, NY 10460 USA. RP Muller-Landau, HC (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA. EM hmuller@umn.edu RI Thomas, Sean/B-6089-2008; Marks, Christian/F-7403-2012; Thompson, Jill/K-2200-2012 OI Thompson, Jill/0000-0002-4370-2593 NR 53 TC 90 Z9 93 U1 4 U2 41 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2006 VL 9 IS 5 BP 589 EP 602 DI 10.1111/j.1461-0248.2006.00915.x PG 14 WC Ecology SC Environmental Sciences & Ecology GA 032UB UT WOS:000236799600009 PM 16643304 ER PT J AU Smith, DR AF Smith, David R. TI A new sawfly genus from India for the "forgotten" Periclista bumasta Konow, 1907 (Hymenoptera : Tenthredinidae) SO ENTOMOLOGICAL NEWS LA English DT Article DE Periclista bumasta; Malkiatus bumastus; new genus; Hymenoptera; Tenthredinidae; India AB Malkiatus, n. gen., subfamily Blennocampinae, is described for Periclista bumasta Konow, 1907, which becomes Malkiatus bumastus (Konow), n. comb. The species is redescribed. Malkiatus includes only the single species from Sikkim, India. C1 Care of Smithsonian Inst, Natl Museum Nat Hist, USDA ARS, Systemat Entomol Lab, Washington, DC 20013 USA. RP Smith, DR (reprint author), Care of Smithsonian Inst, Natl Museum Nat Hist, USDA ARS, Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM dsmith@sel.barc.usda.gov NR 15 TC 2 Z9 2 U1 0 U2 0 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 MAY-JUN PY 2006 VL 117 IS 3 BP 261 EP 264 DI 10.3157/0013-872X(2006)117[261:ANSGFI]2.0.CO;2 PG 4 WC Entomology SC Entomology GA 079BN UT WOS:000240150600002 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI Central questions in the domestication of plants and animals SO EVOLUTIONARY ANTHROPOLOGY LA English DT Article DE domestication; origins of agriculture; plants; animals; climate change; demographic pressure; social forces; Southwest Asia ID NEAR-EAST; UNCONSCIOUS SELECTION; ANCIENT DNA; ORIGINS; AGRICULTURE; EVOLUTION; MAIZE; PLEISTOCENE; TRANSITION; HUSBANDRY AB Along with symbolic communication, tool use, and bipedalism, the domestication of plants and animals, together with the associated emergence of agriculture, stands as one of the pivotal thresholds in human evolution. For more than a hundred years researchers have wrestled with the questions of what domestication is, how it is detected, and why it happened. The past decade in particular has witnessed a remarkable acceleration of interest in domestication, thanks to advances in our ability to detect the context, timing, and process of domestication in a wide array of different plant and animal species around the world.(1) This review focuses on overarching issues of defining, documenting, and explaining the domestication of plants and animals, tracing a path through often discordant viewpoints to offer some new perspectives. C1 Smithsonian Inst, Museum Natl Hist Nat, Archaeobiol Program, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Archaeobiol Program, Washington, DC 20560 USA. NR 98 TC 84 Z9 86 U1 8 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1060-1538 EI 1520-6505 J9 EVOL ANTHROPOL JI Evol. Anthropol. PD MAY-JUN PY 2006 VL 15 IS 3 BP 105 EP 117 DI 10.1002/evan.20101 PG 13 WC Anthropology SC Anthropology GA 062GI UT WOS:000238932200006 ER PT J AU Kirby, KR Laurance, WF Albernaz, AK Schroth, G Fearnside, PM Bergen, S Venticinque, EM da Costa, C AF Kirby, KR Laurance, WF Albernaz, AK Schroth, G Fearnside, PM Bergen, S Venticinque, EM da Costa, C TI The future of deforestation in the Brazilian Amazon SO FUTURES LA English DT Article ID TROPICAL FORESTS; LAND-TENURE; FIRE; CONSERVATION; CONSEQUENCES; ENVIRONMENT; ECONOMICS; PROTECT AB Concern about the future of Amazonian forests is growing as both the extent and rate of primary forest destruction increase. We combine spatial information on various biophysical, dernographic and infrastructural factors in the Brazilian Amazon with satellite data on deforestation to evaluate the relative importance of each factor to deforestation in the region. We assess the sensitivity of results to alternative sampling methodologies, and compare our results to those of previous empirical studies of Amazonian deforestation. Our findings, in concert with those of previous studies. send a clear message to planners: both paved and unpaved roads are key drivers of the deforestation process. Proximity to previous clearings, high population densities, low annual rainfall, and long dry seasons also increase the likelihood that a site will be deforested however, roads are consistently important and are the factors most amenable to policymaking. We argue that there is ample evidence to justify a fundamental change in current Amazonian development priorities if additional largescale losses of forests and environmental services are to be avoided. Published by Elsevier Ltd. C1 Smithsonian Trop Res Inst, Balboa, Panama. McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Museu Goeldi, Belem, Para, Brazil. Conservat Int, Washington, DC 20036 USA. Natl Inst Amazonian Res INPA, Dept Ecol, Manaus, Amazonas, Brazil. Mt Holyoke Coll, Ctr Environm, S Hadley, MA 01075 USA. Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@si.edu RI Kirby, Kathryn/D-1151-2011; Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011; Albernaz, Ana Luisa/K-5226-2012; Venticinque, Eduardo/G-8961-2015 OI Fearnside, Philip/0000-0003-3672-9082; NR 64 TC 79 Z9 87 U1 1 U2 47 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0016-3287 J9 FUTURES JI Futures PD MAY PY 2006 VL 38 IS 4 BP 432 EP 453 DI 10.1016/j.futures.2005.07.011 PG 22 WC Economics; Planning & Development SC Business & Economics; Public Administration GA 026KF UT WOS:000236337100004 ER PT J AU Laurance, WF Alonso, A Lee, M Campbell, P AF Laurance, WF Alonso, A Lee, M Campbell, P TI Challenges for forest conservation in Gabon, central Africa SO FUTURES LA English DT Article ID WILDLIFE POPULATIONS; NORTHEASTERN GABON; TROPICAL FORESTS; CONGO BASIN; RAIN-FOREST; EXTINCTION; IMPACTS; RESERVE; MONKEY; CRISIS AB In recent decades, large expanses of tropical rainforest in central and western Africa have been cleared, logged, fragmented, and overhunted. In contrast, extensive forest in Gabon has survived in a relatively intact condition because the country has a sparse population and substantial petroleum and mineral deposits that have reduced economic pressures on forests. Unfortunately, Gabon's petroleum reserves are dwindling. As a direct result, industrial logging is expanding rapidly; nearly half of the country's forest is currently in timber leases, and this could increase to over 75% of the remaining forest during the next decade. Mechanized logging has important ecological impacts on forests, but the most severe effects are indirect, because loggers create labyrinths of roads that greatly increase access to forests for hunters and slash-and-burn farmers. Declines of forest wildlife from overhunting have been severe in much of tropical Africa, and are likely to rise sharply in Gabon as physical accessibility to forests increases. The Gabonese government is eager to consider afternative strategies to augment economic development, including promotion of an ecotourism industry. This commitment is evidenced by the government's recent designation of 13 new national parks that comprise over a tenth of the country's land area. Efforts to develop ecotourism face substantial challenges, however, including the high profitability of exploitative land uses like logging, the illegal encroachment of loggers and hunters into nature reserves, political instability in the surrounding region, and limited infrastructure for tourism. Nevertheless, these and other efforts to promote more-sustainable development should be strongly supported, as Gabonese forests have among the highest levels of species diversity and endemism in tropical Africa and are likely to play a critical future role in biodiversity conservation. Published by Elsevier Ltd. C1 Smithsonian Trop Res Inst, Balboa, Panama. Monitoring & Assessment Biodivers Program, Washington, DC 20560 USA. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012 NR 56 TC 27 Z9 29 U1 8 U2 33 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0016-3287 J9 FUTURES JI Futures PD MAY PY 2006 VL 38 IS 4 BP 454 EP 470 DI 10.1016/j.futures.2005.07.012 PG 17 WC Economics; Planning & Development SC Business & Economics; Public Administration GA 026KF UT WOS:000236337100005 ER PT J AU Ewers, RM AF Ewers, RM TI Interaction effects between economic development and forest cover determine deforestation rates SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE afforestation; deforestation; economic development; forest cover; GDP; plantation ID ENVIRONMENTAL KUZNETS CURVE; CROSS-COUNTRY ANALYSIS; RESOURCE CURSE; PUERTO-RICO; LAND-USE; BIODIVERSITY CONSERVATION; TROPICAL DEFORESTATION; GLOBAL BIODIVERSITY; ECOSYSTEM SERVICES; OPPORTUNITY COSTS AB Recent work on global patterns of deforestation has shown that countries with high per capita GDP or low remaining forest cover are more likely to be experiencing afforestation than deforestation. Here, I show that the relationship is more complex than previously described, because the effect of one variable is dependent upon the value of the other. As a result, high-income nations exhibit the opposite response to disappearing forest cover than low-income nations. In an analysis of 103 countries, I found that high-income countries with low forest cover have the highest rates of afforestation, typically through the establishment of new plantations. In contrast, low-income countries with little forest are more likely to consume that remaining portion at a faster proportional rate than do low-income countries with more forest. Nations with large amounts of forest have approximately equal deforestation rates, regardless of national wealth. These results highlight for the first time that there is a strong interaction between forest cover and economic development that determines rates of forest change among nations. (C) 2006 Elsevier Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Ewers, RM (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM robert.ewers@ioz.ac.uk NR 83 TC 41 Z9 46 U1 8 U2 34 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD MAY PY 2006 VL 16 IS 2 BP 161 EP 169 DI 10.1016/j.gloenvcha.2005.12.001 PG 9 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA 051NM UT WOS:000238167800005 ER PT J AU Froidevaux, L Livesey, NJ Read, WG Jiang, YBB Jimenez, C Filipiak, MJ Schwartz, MJ Santee, ML Pumphrey, HC Jiang, JH Wu, DL Manney, GL Drouin, BJ Waters, JW Fetzer, EJ Bernath, PF Boone, CD Walker, KA Jucks, KW Toon, GC Margitan, JJ Sen, B Webster, CR Christensen, LE Elkins, JW Atlas, E Lueb, RA Hendershot, R AF Froidevaux, L Livesey, NJ Read, WG Jiang, YBB Jimenez, C Filipiak, MJ Schwartz, MJ Santee, ML Pumphrey, HC Jiang, JH Wu, DL Manney, GL Drouin, BJ Waters, JW Fetzer, EJ Bernath, PF Boone, CD Walker, KA Jucks, KW Toon, GC Margitan, JJ Sen, B Webster, CR Christensen, LE Elkins, JW Atlas, E Lueb, RA Hendershot, R TI Early validation analyses of atmospheric profiles from EOS MLS on the Aura satellite SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE atmospheric retrievals; data validation ID HALOGEN OCCULTATION EXPERIMENT; DATA SET; SPECTROMETER; AIRS/AMSU/HSB; BALLOON; SYSTEM AB We present results of early validation studies using retrieved atmospheric profiles from the Earth Observing System Microwave Limb Sounder (MLS) instrument on the Aura satellite. "Global" results are presented for MLS measurements of atmospheric temperature, ozone, water vapor, hydrogen chloride, nitrous oxide, nitric acid, and carbon monoxide, with a focus on the January-March 2005 time period. These global comparisons are made using long-standing global satellites and meteorological datasets, as well as some measurements from more recently launched satellites. Comparisons of MLS data with measurements from the Ft. Sumner, NM, September 2004 balloon flights are also presented. Overall, good agreement is obtained, often within 5% to 10%, but we point out certain issues to resolve and some larger systematic differences; some artifacts in the first publicly released MLS (version 1.5) dataset are noted. We comment briefly on future plans for validation and software improvements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Edinburgh, Edinburgh EH9 3JN, Midlothian, Scotland. Univ Waterloo, Waterloo, ON N2L 3G1, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Ocean & Atmospher Adm, Climate Monitoring & Diagnost Lab, Boulder, CO 80305 USA. Univ Miami, Miami, FL 33149 USA. Natl Ctr Atmospher Res, Boulder, CO 80303 USA. New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lucien@mls.jpl.nasa.gov RI Bernath, Peter/B-6567-2012; Atlas, Elliot/J-8171-2015; Schwartz, Michael/F-5172-2016; Wu, Dong/D-5375-2012 OI Bernath, Peter/0000-0002-1255-396X; Schwartz, Michael/0000-0001-6169-5094; NR 45 TC 168 Z9 170 U1 2 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAY PY 2006 VL 44 IS 5 BP 1106 EP 1121 DI 10.1109/TGRS.2006.864366 PG 16 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 037SK UT WOS:000237167100006 ER PT J AU Gingerich, O AF Gingerich, O TI Supplement to the Copernican Census SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2006 VL 37 BP 232 EP 232 PN 2 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 038AU UT WOS:000237190600008 ER PT J AU Cook, DE Kovacevich, B Beach, T Bishop, R AF Cook, DE Kovacevich, B Beach, T Bishop, R TI Deciphering the inorganic chemical record of ancient human activity using ICP-MS: a reconnaissance study of late Classic soil floors at Cancuen, Guatemala SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE soil chemistry; ICP-MS; geoarchaeology; anthrosol; heavy metals; Guatemala; Maya ID RARE-EARTH-ELEMENTS; MULTIELEMENTAL CHARACTERIZATION; PIEDRAS NEGRAS; HOUSE FLOORS; PHOSPHORUS; SIGNATURES; EROSION; SAMPLES; PRESERVATION; SEDIMENTS AB Inorganic chemical analysis of soil floors using inductively coupled plasma-mass spectrometry (ICP-MS) was undertaken to provide information on the nature and location of past human activity in the ancient Maya city of Cancuen, Guatemala. The use of ICP-MS to detect trace and ultra-trace elemental enrichment of two excavated soil floors from the late Classic period is the first study of its kind in Mesoamerican archaeology. Geochemical background of the site was established by the analysis of palaeosols and nearby undisturbed 'off-site' soil profiles. Robust statistical methods used in the study clearly distinguished the level of anthropogenic enrichment across the former floors. Many elements measured showed only minor departures (10-20%) from the site's background soil chemistry. The greatest levels of elemental enrichment were detected in the rare earth elements, mercury, and gold. The latter is of particular interest considering the consensus that gold was absent from the world of the Classic-period Maya. Comparisons of the spatial pattern of mercury enrichment with lithic and archaeological data show strong linkages to past industrial and ritual activities. Elevated rare earth element concentrations were recorded broadly across both soil floors and are considered to be related to concentrated human occupation in antiquity. Published by Elsevier Ltd. C1 Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. Vanderbilt Univ, Dept Anthropol, Nashville, TN 37235 USA. Georgetown Univ, STIA, Sch Foreign Serv, Washington, DC 20057 USA. Smithsonian Inst, Natl Museum Amer Hist, Div Archaeol, Dept Anthropol, Washington, DC 20560 USA. RP Cook, DE (reprint author), Univ Sydney, Sch Geosci, Madsen Bldg F09, Sydney, NSW 2006, Australia. EM duncanc@mail.usyd.edu.au OI Cook, Duncan/0000-0001-5270-4569 NR 64 TC 30 Z9 31 U1 0 U2 18 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAY PY 2006 VL 33 IS 5 BP 628 EP 640 DI 10.1016/j.jas.2005.09.019 PG 13 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 033SM UT WOS:000236869500003 ER PT J AU Hawkins, BA Diniz, JAF Jaramillo, CA Soeller, SA AF Hawkins, BA Diniz, JAF Jaramillo, CA Soeller, SA TI Post-Eocene climate change, niche conservatism, and the latitudinal diversity gradient of New World birds SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE climate change; evolutionary time; extinction; latitudinal gradient; mean root distance; New World birds; palaeoclimate; species diversity; species ID GLOBALLY CONSISTENT RELATIONSHIP; AVIAN SPECIES RICHNESS; GEOGRAPHIC PATTERNS; TAXON RICHNESS; NORTH-AMERICA; SOUTH-AMERICA; EOCENE; SCALE; EVOLUTIONARY; ANGIOSPERMS AB Aim The aim of this study was to test a variant of the evolutionary time hypothesis for the bird latitudinal diversity gradient derived from the effects of niche conservatism in the face of global climate change over evolutionary time. Location The Western Hemisphere. Methods We used digitized range maps of breeding birds to estimate the species richness at two grain sizes, 756 and 12,100 km(2). We then used molecular phylogenies resolved to family to quantify the root distance (RD) of each species as a measure of its level of evolutionary development. Birds were classified as 'basal' or 'derived' based on the RD of their family, and richness patterns were contrasted for the most basal and most derived 30% of species. We also generated temperature estimates for the Palaeogene across the Western Hemisphere to examine how spatial covariation between past and present climates might make it difficult to distinguish between ecological and evolutionary hypotheses for the current richness gradient. Results The warm, wet tropics support many species from basal bird clades, whereas the northern temperate zone and cool or dry tropics are dominated by species from more recent, evolutionarily derived clades. Furthermore, crucial to evaluating how niche conservatism among birds may drive the hemispherical richness gradient, the spatial structure of the richness gradient for basal groups is statistically indistinguishable from the overall gradient, whereas the richness gradient for derived groups is much shallower than the overall gradient. Finally, modern temperatures and the pattern of climate cooling since the Eocene are indistinguishable as predictors of bird species richness. Main conclusions Differences in the richness gradients of basal vs. derived clades suggest that the hemispherical gradient has been strongly influenced by the differential extirpation of species in older, warm-adapted clades from parts of the world that have become cooler in the present. We propose that niche conservatism and global-scale climate change over evolutionary time provide a parsimonious explanation for the contemporary bird latitudinal diversity gradient in the New World, although dispersal limitation of some highly derived clades probably plays a secondary role. C1 Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. Univ Fed Goias, ICB, Dept Biol Geral, Goiania, Go, Brazil. Univ Catolica Goias, MCAS PROPE, Dept Biol, Goiania, Go, Brazil. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. Univ Calif Irvine, Network Serv, Irvine, CA USA. Univ Calif Irvine, Acad Comp Serv, Irvine, CA USA. RP Hawkins, BA (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. EM bhawkins@uci.edu RI Hawkins, Bradford/A-3510-2011; Diniz-Filho, Jose Alexandre/D-9405-2013 OI Diniz-Filho, Jose Alexandre/0000-0002-0967-9684 NR 59 TC 130 Z9 137 U1 2 U2 55 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD MAY PY 2006 VL 33 IS 5 BP 770 EP 780 DI 10.1111/j.1365-2699.2006.01452.x PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 034PM UT WOS:000236943100002 ER PT J AU Stanley, JD So, VL AF Stanley, JD So, VL TI Inconsistent grain roundness and sphericity trends and the valley wall influx factor: Between Alpine source and lake shore, SE France SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE abrasion; Alps; Annecy Lake; bedload; carbonate grains; fan-delta; lateral influx; proximal settings; sediment failure; texture; transport processes; valley wall sedimentation ID SEDIMENTS; ANNECY AB The greatest change in particle roundness, sphericity, and size in most fluvial systems generally occurs in the initial first few kilometers of sediment transport. Observations in natural settings and laboratory experiments have shown that changes, such as increased grain rounding and decreased size due to particle breakage, wear, and attrition, tend to be progressive along the dispersal path. In marked contrast, this study records highly variable and poorly developed particle-texture trends downslope along short (< 5 km) channels that extend directly from a high-relief carbonate source area down to the shore of Lake Annecy in the western Alps, SE France. The observed inconsistent patterns are measured in both a region-wide analysis using all collected samples and also in a more specific survey of samples in six different channels incised on the steep, topographically irregular mountain flanks that border the lake. The major factor responsible for the irregular downslope patterns of roundness, sphericity, and size in the Annecy study area is the lateral introduction of sediment into the fluvial channels along dispersal paths. Episodic failure of mechanically unstable sediments and their transport down steep valley walls bring less-abraded sediment of variable shape and size along the dispersal paths. The valley wall sediment influx factor warrants further examination to better interpret sedimentation processes in dissected, high-gradient terrains that border coastal areas. C1 Smithsonian Inst, Geoarchaeol Program, NMNH E206, Washington, DC 20013 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Geoarchaeol Program, NMNH E206, Washington, DC 20013 USA. EM Stanley.daniel@nmnh.si.edu NR 16 TC 2 Z9 2 U1 1 U2 2 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD MAY PY 2006 VL 22 IS 3 BP 547 EP 560 DI 10.2112/05A-0022.1 PG 14 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 043PV UT WOS:000237614500007 ER PT J AU Richter, S Kornicker, LS AF Richter, S Kornicker, LS TI The mandibles of a halocyprid ostracode (Halocypridina : Halocypridae) - A new record of mandibular gnathal edges with a "laconia mobilis" SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB A structure resembling the lacinia mobilis in Peracarida (Malacostraca) is described for the coxal gnathal edge of the mandibles in the halocyprid ostracode Spelaeoecia capax. The lacinia mobilis is present at the distal portion of the gnathal edge close to and articulated with the incisor process. Proximal and closely associated with the lacinia, two processes are present. In the center of the gnathal edge, a flat process partly covers two comb-like spines. A molar process (masticatory pad) is present at the proximal end of the gnathal edge. The lacinia mobilis described herein resembles the peracarid lacinia in possessing a number of cusps similar to the cusps of the incisor process, its orientation parallel to the incisor process and the presence of an articular condyle at the basis of the lacinia. The described similarities, however, concern only the left mandible of certain Peracarida where the mandibles are asymmetrical. In Spelaeoccia capax. the mandibles are symmetrical. The lacinia mobilis in certain ostracodes may have evolved independently from that in Peracarida. The term lacinia mobilis is used as a descriptive term only, not implying homology. C1 Univ Jena, Inst Spezielle Zool & Evolut Biol, D-07743 Jena, Germany. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA. RP Richter, S (reprint author), Univ Jena, Inst Spezielle Zool & Evolut Biol, Erbertstr 1, D-07743 Jena, Germany. EM richter.stefan@uni-jena.de; kornickl@si.edu RI Richter, Stefan/E-6256-2012 NR 18 TC 8 Z9 9 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2006 VL 26 IS 2 BP 113 EP 118 DI 10.1651/S-2636.1 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 044HZ UT WOS:000237664300002 ER PT J AU Eberhard, W AF Eberhard, W TI Sexually antagonistic coevolution in insects is associated with only limited morphological diversity SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Review DE female choice; sexually antagonistic coevolution; sexual morphology; sexual selection ID DIVING BEETLES COLEOPTERA; LUCILIA-CUPRINA FEMALES; BOREAL WATER BEETLE; TRAUMATIC INSEMINATION; FUNCTIONAL-MORPHOLOGY; MATE CHOICE; GLOSSINA-PALLIDIPES; HEMIPTERA GERRIDAE; AQUARIUS-REMIGIS; MATING-BEHAVIOR AB Morphological traits involved in male-female sexual interactions, such as male genitalia, often show rapid divergent evolution. This widespread evolutionary pattern could result from sustained sexually antagonistic coevolution, or from other types of selection such as female choice or selection for species isolation. I reviewed the extensive but under-utilized taxonomic literature on a selected subset of insects, in which male-female conflict has apparently resulted in antagonistic coevolution in males and females. I checked the sexual morphology of groups comprising 500-1000 species in six orders for three evolutionary trends predicted by the sexually antagonistic coevolution hypothesis: males with species-specific differences and elaborate morphology in structures that grasp or perforate females in sexual contexts; corresponding female structures with apparently coevolved species-specific morphology; and potentially defensive designs of female morphology. The expectation was that the predictions were especially likely to be fulfilled in these groups. A largely qualitative overview revealed several surprising patterns: sexually antagonistic coevolution is associated with frequent, relatively weak species-specific differences in males, but male designs are usually relatively simple and conservative (in contrast to the diverse and elaborate designs common in male structures specialized to contact and hold females in other species, and also in weapons such as horns and pincers used in intra-specific battles); coevolutionary divergence of females is not common; and defensive female divergence is very uncommon. No cases were found of female defensive devices that can be facultatively deployed. Coevolutionary morphological races may have occurred between males and females of some bugs with traumatic insemination, but apparently as a result of female attempts to control fertilization, rather than to reduce the physical damage and infections resulting from insertion of the male's hypodermic genitalia. In sum, the sexually antagonistic coevolution that probably occurs in these groups has generally not resulted in rapid, sustained evolutionary divergence in male and female external sexual morphology. Several limitations of this study, and directions for further analyses are discussed. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Eberhard, W (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 144 TC 33 Z9 34 U1 4 U2 28 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD MAY PY 2006 VL 19 IS 3 BP 657 EP 681 DI 10.1111/j.1420-9101.2005.01057.x PG 25 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 034PL UT WOS:000236943000001 PM 16674564 ER PT J AU Yanoviak, SP Dudley, R AF Yanoviak, SP Dudley, R TI The role of visual cues in directed aerial descent of Cephalotes atratus workers (Hymenoptera : Formicidae) SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE ant; Cephalotes atratus; behavior; color; gliding; orientation; tropical forest ID COLOR; FORESTS; CANOPY; LIGHT; ANTS AB Animals often depend on properties of reflected light (e. g. color, brightness) to locate resources. We compared reflectance properties of tree trunks with surrounding vegetation, and examined how differences in reflectance profiles of surrogate tree trunks (red, yellow, green, blue, black, gray, dark gray and white sheets) affected the directed aerial descent of worker Cephalotes atratus (L.) ants. Across the visual spectrum, tree trunk reflectance was 2-10 times higher than the surrounding foliage and differed among trees. In two separate experiments, one with colored sheets and one with black, white and gray sheets, nearly half (42% and 47%, respectively) of falling ants directed their descent to a bright white sheet when given a choice of target colors or shades of gray. When colored and gray sheets were presented individually, landing frequencies were lower than expected for all except white sheets. Glide performance was highly variable, but there was a tendency for higher glide indices to be associated with the white sheet relative to the green sheet. We conclude that visually mediated aerial behavior in falling canopy ants is strongly influenced by reflectance properties of the target object, specifically brightness, and correlates with preferred natural targets of tree trunks. C1 Univ Texas, Med Branch, Dept Pathol, Galveston, TX 77555 USA. Florida Med Entomol Lab, Vero Beach, FL 32962 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Yanoviak, SP (reprint author), Univ Texas, Med Branch, Dept Pathol, Galveston, TX 77555 USA. EM syanoviak@yahoo.com FU NIAID NIH HHS [AI049725] NR 19 TC 23 Z9 24 U1 0 U2 9 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD MAY 1 PY 2006 VL 209 IS 9 BP 1777 EP 1783 DI 10.1242/jeb.02170 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 038LC UT WOS:000237220300030 PM 16621958 ER PT J AU Capper, A Tibbetts, IR O'Neil, JM Shaw, GR AF Capper, A Tibbetts, IR O'Neil, JM Shaw, GR TI Feeding preference and deterrence in rabbitfish Siganus fuscescens for the cyanobacterium Lyngbya majuscula in Moreton Bay, south-east Queensland, Australia SO JOURNAL OF FISH BIOLOGY LA English DT Article DE chemical deterrence; debromaplysiatoxin; lyngbyatoxin-a; Siganidae; top-down control ID MARINE NATURAL-PRODUCTS; SECONDARY METABOLITES; CHEMICAL DEFENSES; JUVENILE RABBITFISH; FOOD; SEA; TOXINS; GUAM; APLYSIATOXINS; DERMATITIS AB Rabbitfish Siganus fuscescens preferences for Lyngbya majuscula collected from three bloom locations in Moreton Bay, Queensland, Australia, were tested along with a range of local plant species in the laboratory. Consumption of L. majuscula by fish did not differ between wild and captive-bred fish (P = 0.152) but did differ between bloom location (P = 0.039). No relationship was found between consumption rates and lyngbyatoxin-a concentration (r(2) = 0.035, P = 0.814). No correlation existed between C : N and proportion of food consumed when all food types were analysed statistically, whereas a clear correlation was observed when L. majuscula was removed from the calculations. In simulated bloom conditions, fish avoided ingestion of L. majuscula by feeding through gaps in the L. majuscula coverage. Both wild and captive-bred S. fuscescens showed a distinct feeding pattern in 10 day no-choice feeding assays, with less L. majuscula being consumed than the preferred red alga Acanthophora spicifera. Lyngbya majuscula however, was consumed in equal quantities to A. spicifera by wild S. fuscescens when lyngbyatoxin-a was not detectable. Wild fish probably do not preferentially feed on L. majuscula when secondary metabolites are present and are not severely impacted by large L. majuscula blooms in Moreton Bay. Furthermore, poor feeding performance in both captive-bred and wild S. fuscescens suggests that they would exert little pressure as a top-down control agent of toxic L. majuscula blooms within Moreton Bay. (c) 2006 The Fisheries Society of the British Isles. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. Univ Queensland, Sch Life Sci, Ctr Marine Studies, Brisbane, Qld 4072, Australia. Univ Maryland, Ctr Environm Sci, Cambridge, MD 21673 USA. Univ Queensland, Natl Ctr Environm Toxicol EnTox, Coopers Plains, Qld 4108, Australia. RP Capper, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM capper@sms.si.edu RI Capper, Angela/B-4403-2012; Tibbetts, Ian/K-6191-2013; O'Neil, Judith/F-9024-2013; OI Tibbetts, Ian/0000-0002-1481-238X; O'Neil, Judith/0000-0002-7697-5299; Capper, Angela/0000-0002-4922-0253 NR 50 TC 13 Z9 14 U1 0 U2 15 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD MAY PY 2006 VL 68 IS 5 BP 1589 EP 1609 DI 10.1111/j.1095-8649.2006.01048.x PG 21 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 040ZK UT WOS:000237422200020 ER PT J AU Ubelaker, DH Buchholz, BA Stewart, JEB AF Ubelaker, DH Buchholz, BA Stewart, JEB TI Analysis of artificial radiocarbon in different skeletal and dental tissue types to evaluate date of death SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; radiocarbon; skeletons; date of death; bomb-curve ID BOMB C-14; BONE; CALIBRATION; TURNOVER; TEETH; AMS AB Radiocarbon dating, with special reference to the modern bomb-curve, can provide useful information to elucidate the date of death of skeletonized human remains. Interpretation can be enhanced with analysis of different types of tissues within a single skeleton because of the known variability of formation times and remodeling rates. Analysis of radiocarbon content of teeth, especially the enamel in tooth crowns, provides information about the date of formation in the childhood years and in consideration of the known timing of tooth formation can be used to estimate the birth date after 1950 AD. Radiocarbon analysis of modern cortical and trabecular bone samples from the same skeleton may allow proper placement on the pre-1963 or post-1963 sides of the bomb-curve as most trabecular bone generally undergoes more rapid remodeling than does most cortical bone. Pre-1963 bone formation would produce higher radiocarbon values for most trabecular bone than for most cortical bone. This relationship is reversed for formation after 1963. Radiocarbon analysis was conducted in this study on dental, cortical, and trabecular bone samples from two adult individuals of known birth (1925 and 1926) and death dates (1995 and 1959). As expected, the dental results correspond to prebomb-curve values reflecting conditions during the childhoods of the individuals. The radiocarbon content of most bone samples reflected the higher modern bomb-curve values. Within the bone sample analyses, the values of the trabecular bone were higher than those of cortical bone and supported the known placement on the pre-1963 side of the bomb-curve. C1 Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. Lawrence Livermore Natl Lab, Ctr Accelerator Mass Spectrometry, Livermore, CA 94551 USA. Natl Missing Person DNA Database, DNA Anal Unit 2, FBI Lab, Quantico, VA 22135 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, NMNH, Dept Anthropol, MRC 112, Washington, DC 20560 USA. EM ubelaked@si.edu RI Buchholz, Bruce/G-1356-2011 NR 26 TC 36 Z9 38 U1 2 U2 24 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAY PY 2006 VL 51 IS 3 BP 484 EP 488 DI 10.1111/j.1556-4029.2006.00125.x PG 5 WC Medicine, Legal SC Legal Medicine GA 040QM UT WOS:000237395500004 PM 16696693 ER PT J AU Hershler, R Liu, HP Frest, TJ Johannes, EJ Clark, WH AF Hershler, R Liu, HP Frest, TJ Johannes, EJ Clark, WH TI Genetic structure of the western North American aquatic gastropod genus Taylorconcha and description of a second species SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID MOLECULAR SYSTEMATICS; DNA; CONSERVATION; RISSOOIDEA; SUBSTITUTION; HYDROBIIDAE; EVOLUTION; TREES; MODEL AB The Bliss Rapids Snail (Taylorconcha serpenticola) is a threatened species that ranges along a short reach of the middle Snake River in southern Idaho. Additional Taylorconcha populations of uncertain taxonomic status have recently been discovered in other portions of the Snake River basin (Owyhee River, lower Snake River). We investigated the phylogenetic relationships and population structure of these snails, together with two outgroups, using cytochrome c oxidase subunit I (COI) of mitochondrial DNA and the first internal transcribed spacer region between the 18S and 5.8S ribosomal DNA. These data show no sharing of haplotypes or genotypes among T. serpenticola and the Owyhee-Lower Snake populations, with both depicted as monophyletic units within the Taylorconcha clade. Both of these datasets and morphological evidence suggest that the Owyhee-Lower Snake populations are a distinct species, which we describe herein (T. insperata new species). Application of an available COI molecular clock suggests that Taylorconcha arose in the late Miocene, when ancestral Snake River drainage was impounded in an extensive lacustrine system ('Lake Idaho') in western Idaho. The shallow population structuring of T. insperata suggests that the lower Snake River was only recently colonized subsequent to incision of Hells Canyon, draining of Lake Idaho, and development of a through-going river in the late Neogene. The absence of significant genetic structure in T. serpenticola, which is attributed to the unstable course and flow regime of the middle Snake River during the Quaternary, suggests that this species can be treated as a single management unit. C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Denver, Dept Biol Sci, Denver, CO 80208 USA. DEIXIS Consultants, Seattle, WA 98115 USA. Idaho Power Co, Boise, ID 83702 USA. Albertson Coll Idaho, Orma J Smith Museum Nat Hist, Caldwell, ID 83605 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305 MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu NR 42 TC 10 Z9 10 U1 2 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 J9 J MOLLUS STUD JI J. Molluscan Stud. PD MAY PY 2006 VL 72 BP 167 EP 177 DI 10.1093/mollus/eyi066 PN 2 PG 11 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 039QJ UT WOS:000237321000007 ER PT J AU Touwaide, A AF Touwaide, Alain TI The kidney from Galen to Vesalius - A first approach SO JOURNAL OF NEPHROLOGY LA English DT Article; Proceedings Paper CT 5th Congress of International-Association-for-the-History-of-Nephrolgoy CY APR 13-15, 2005 CL Gdansk, POLAND SP Int Assoc Hist Nephrol DE Vesalius; Galen; dissection; classical tradition; Renaissance AB In 1543, Andreas Vesalius (1514 - ca. 1564) published de Humani corporisfabrica in Basel (Basel, 1543). In current literature, the work is interpreted as either an imitation or a refutation of previous anatomical knowledge, particularly the treatises by the classical Greek physician Galen (129 - after 216 A.D. [?]). In this paper we focus on Vesalius' study of the kidneys (Book V, chapter 10). On the basis of a comparison of Vesalius' and Galen's Greek text, we reach the conclusion that Vesalius closely reproduced Galen's model and text, thus reenacting the ancient practice of medicine and dissection. C1 Natl Museum Natl Hist, Dept Bot MRC 166, Smithsonian Inst, Washington, DC 20013 USA. RP Touwaide, A (reprint author), Natl Museum Natl Hist, Dept Bot MRC 166, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM TouwaideA@si.edu NR 18 TC 0 Z9 0 U1 0 U2 0 PU WICHTIG EDITORE PI MILAN PA 72/74 VIA FRIULI, 20135 MILAN, ITALY SN 1121-8428 J9 J NEPHROL JI J. Nephrol. PD MAY-JUN PY 2006 VL 19 SU 10 BP S4 EP S8 PG 5 WC Urology & Nephrology SC Urology & Nephrology GA 065PU UT WOS:000239172600002 PM 16874707 ER PT J AU Hoare, RD Pojeta, J AF Hoare, RD Pojeta, J TI Ordovician polyplacophora (mollusca) from North America SO JOURNAL OF PALEONTOLOGY LA English DT Review ID PALEOZOIC POLYPLACOPHORA; EARLY HISTORY; GOTLAND; CHITONS; SWEDEN; DIVERSIFICATION; CHELODES; TEXAS AB Abundant silicified polyplacophorans from numerous localities in the Ordovician in Kentucky and other localities in Virginia, Wisconsin, and Minnesota are described systematically. New species are: Spicuchelodes cressmani, Calceochiton floweri. Preacanthochilon baueri, Orthriochiton recavus, Helminthochiton blacki. H. marginatus, and Alastega martini; new genera and species are: Listrochiton weiri, Litochiton crebatus, and Amblytochiton incomptus; and new families are Litochitonidae and Alastegiidae. Hemithecella expansa Ulrich and Bridge in Butts. 1941 and Chelodes cf. C. mirabilis (Butts, 1926). from the Chepultepec Formation in Virginia are also described. Comparisons are made with Chelodes whitehousei Runneggar, Pojeta, Taylor, and Collins, 1979 from Australia and Calceochiton hachitae Flower, 1968 from New Mexico. C1 Bowling Green State Univ, Dept Geol, Bowling Green, OH 43403 USA. Smithsonian Inst, Natl Museum Nat Hist, US Geol Survey, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Hoare, RD (reprint author), Bowling Green State Univ, Dept Geol, Bowling Green, OH 43403 USA. NR 125 TC 6 Z9 6 U1 0 U2 1 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 MAY PY 2006 VL 80 IS 3 SU S BP 1 EP 27 DI 10.1666/0022-3360(2006)80[1:OPMFNA]2.0.CO;2 PG 27 WC Paleontology SC Paleontology GA 037EK UT WOS:000237129300001 ER PT J AU Kiel, S AF Kiel, S TI New and little-known gastropods from the Albian of the Mahajanga Basin, northwestern Madagascar SO JOURNAL OF PALEONTOLOGY LA English DT Review ID HETEROBRANCHIA; PROSOBRANCHIA; SYSTEMATICS; MOLLUSCA; ANATOMY; MORPHOLOGY; PHYLOGENY; GENERA AB Thirty-one gastropod species and one type of isolated larval shell are described from a quarry near Ambatolafia in the Mahajanga Basin, northwestern Madagascar. The ammonite fauna indicates a lower Albian age of the fauna (Cleoniceras besairiei Zone). The taxonomic position of the species described earlier is reviewed, incorporating new data on shell structure and protoconch morphology. Twelve species and one genus are new, with four species described in open nomenclature. The oldest hitherto known representatives of Cocculina sensu late, lphitus, Conjectura, Entomope, Tomura. and possibly Vatopsis and Paladmete, are described. Nacre is documented in a species of Semisolarium, providing further evidence for the position of this genus within the Vetigastropoda. Eight of the species occur also in the Cretaceous of Europe or are tentatively assigned to European species. Three species have close relatives in the Aptian/Albian of Japan, one species may have relations to the Albian of Texas. The new genus is Mahajangina (family uncertain) for a species having a small, trochispiral teleoconch with spines on the periphery, and a conical. bicarinate larval shell. The new species are: Cirsocerithium collignoni, Zardinistylus betsibokaensis, Pommerozygia mahajangensis, Conjectura minuta, Buvignieria benvaldi, Mahajangina weitschati. Entomope crassilabrion, Paladmete? rasoarinoroae, Tomura anibatolafiensis, Carinathilda parviruga, Carinathilda bandeli, and Gymnothilda pagodoidea. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Paleobiol MRC 121, Washington, DC 20013 USA. RP Kiel, S (reprint author), Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. EM kiels@si.edu RI Kiel, Steffen/C-3150-2009 OI Kiel, Steffen/0000-0001-6281-100X NR 151 TC 21 Z9 25 U1 0 U2 1 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 MAY PY 2006 VL 80 IS 3 BP 455 EP 476 DI 10.1666/0022-3360(2006)80[455:NALGFT]2.0.CO;2 PG 22 WC Paleontology SC Paleontology GA 035ZZ UT WOS:000237041700005 ER PT J AU Sanmartin, JR Estes, RD Lorenzini, EC Elaskar, SA AF Sanmartin, J. R. Estes, R. D. Lorenzini, E. C. Elaskar, S. A. TI Efficiency of electrodynamic tether thrusters SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 7th International Conference on Protection of Materials and Structures from Space Environment (ICPMSE-7) CY 2004 CL Toronto, CANADA ID CYLINDRICAL LANGMUIR PROBES; MOTION-LIMITED REGIME; PROPULSION; SYSTEMS AB The performance efficiency of electrodynamic bare tethers acting as thrusters in low Earth orbit, as gauged by the ratio of the system mass dedicated to thrust over mission impulse, is analyzed and compared to the performance efficiency of electrical thrusters. Tether systems are much lighter for times beyond six months in space-tug operations, where there is a dedicated solar array, and beyond one month for reboost of the International Space Station, where the solar array is already in place. Bare-tether propulsive efficiency itself, with the tether considered as part of the power plant, is higher for space tugs. Tether optimization shows that thin tapes have greater propulsive efficiency and are less sensitive to plasma density variations in orbit than cylindrical tethers. The efficiency increases with tape length if some segment next to the power supply at, the top is insulated to make the tether potential bias vanish at the lower end; multitape tethers must be used to keep the efficiency high at high thrust levels. The efficiency has a maximum for tether-hardware mass equal to the fraction of power-subsystem mass going into ohmic power, though the maximum is very flat. For space tugs, effects of induced-bias changes in orbit might need to be reduced by choosing a moderately large power-subsystem to tether-hardware mass ratio or by tracking the current-voltage characteristic of the solar array. C1 Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, Dept Fis, E-28040 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Geoastron Div, Cambridge, MA 02138 USA. Univ Nacl Cordoba, Consejo Nacl Invest Cient & Tecn, Dept Aeronaut, RA-2000 Cordoba, Argentina. RP Sanmartin, JR (reprint author), Univ Politecn Madrid, Escuela Tecn Super Ingn Aeronaut, Dept Fis, Pza C Cisneros 3, E-28040 Madrid, Spain. NR 14 TC 8 Z9 12 U1 0 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAY-JUN PY 2006 VL 43 IS 3 BP 659 EP 666 DI 10.2514/1.16174 PG 8 WC Engineering, Aerospace SC Engineering GA 055SM UT WOS:000238470700028 ER PT J AU Stapley, J AF Stapley, J TI Individual variation in preferred body temperature covaries with social behaviours and colour in male lizards SO JOURNAL OF THERMAL BIOLOGY LA English DT Article DE aggression; courtship; behavioural syndromes; individual variation; Pseudemoia entrecasteauxii; metabolic rate; thermoregulation; conflicting selection; personalities; shy-bold ID ANTIPREDATOR BEHAVIOR; PHYSIOLOGICAL PERFORMANCE; SCELOPORUS-MERRIAMI; TERRITORIAL DEFENSE; EULAMPRUS-TYMPANUM; THERMAL PHYSIOLOGY; METABOLIC-RATE; RAINBOW-TROUT; MALE-MICE; AGGRESSION AB I. I tested if individual variation in preferred body temperature (PBT) covaried with behaviours and male phenotypic traits (size and colouration) in Pseudemoia entrecasteauxii. 2. Individuals varied in their PBT and this variation was repeatable across days. PBT was not related to body size but males with orange ventral colour had higher PBT. 3. Males with orange ventral colour were more aggressive and dominated males with white venters. 4. Male behaviours were correlated and they covaried with PBT. Correlated behaviours such as these may be related to a shy-bold continuum. (c) 2006 Elsevier Ltd. All rights reserved. C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT, Australia. RP Stapley, J (reprint author), Smithsonian Trop Res Inst, Unit 4098, APO, AA 34002 USA. EM stapleyj@si.edu RI Stapley, Jessica/B-3858-2010 NR 52 TC 20 Z9 21 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0306-4565 J9 J THERM BIOL JI J. Therm. Biol. PD MAY PY 2006 VL 31 IS 4 BP 362 EP 369 DI 10.1016/j.jtherbio.2006.01.008 PG 8 WC Biology; Zoology SC Life Sciences & Biomedicine - Other Topics; Zoology GA 037TV UT WOS:000237171000013 ER PT J AU Clarke, AC Burtenshaw, MK McLenachan, PA Erickson, DL Penny, D AF Clarke, AC Burtenshaw, MK McLenachan, PA Erickson, DL Penny, D TI Reconstructing the origins and dispersal of the polynesian bottle gourd (Lagenaria siceraria) SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article; Proceedings Paper CT 3rd Society-for-Molecular-Biology-and-Evolution Young Investigators Workshop (SMBEYI-3) CY JUN 24-27, 2005-2006 CL Palmerston, NEW ZEALAND SP Soc Mol Biol & Evolut DE Lagenaria siceraria; bottle gourd; Polynesia; human migration; crop domestication; ISSR; SCAR markers ID PACIFIC; DOMESTICATION; SEQUENCE; PLANT; AMPLIFICATION; MIGRATIONS; SUPPORT; HISTORY; ISLAND AB The origin of the Polynesian bottle gourd (Lagenaria siceraria), an important crop species in prehistoric Polynesia, has remained elusive. Most recently, a South American origin has been favored as the bottle gourd could have been introduced from this continent with the sweet potato by Polynesian voyagers around A.D. 1,000. To test the hypothesis of an American origin for the Polynesian bottle gourd, we developed seven markers specific to bottle gourd (two chloroplast and five nuclear). The nuclear markers were developed using a new technique where polymorphic inter simple sequence repeat (ISSR) markers are converted into single-locus polymerase chain reaction and sequencing markers-an approach that will be useful for developing markers in other taxa. All seven markers were sequenced in 36 cultivars of bottle gourd from Asia, the Americas, and Polynesia. The results support a dual origin for the Polynesian bottle gourd: the chloroplast markers are exclusively of Asian origin, but the nuclear markers show alleles originating in both the Americas and Asia. Because hybridization of Polynesian bottle gourds with post-European introductions cannot be excluded, ancient DNA from archaeological material will be useful for further elucidating the prehistoric movements of this species in Polynesia. This work has implications not only for the dispersal of the Polynesian bottle gourd but also for the domestication and dispersal of the species as a whole. C1 Massey Univ, Allan Wilson Ctr Mol Ecol & Evolut, Palmerston North, New Zealand. Massey Univ, Inst Mol BioSci, Palmerston North, New Zealand. Open Polytech New Zealand, Nat Resource Ctr, Lower Hutt, New Zealand. Smithsonian Inst, Museum Natl Hist Nat, Labs Analyt Biol, Washington, DC 20560 USA. RP Clarke, AC (reprint author), Massey Univ, Allan Wilson Ctr Mol Ecol & Evolut, Palmerston North, New Zealand. EM a.c.clarke@massey.ac.nz RI Clarke, Andrew/A-7635-2008; Penny, David/E-9410-2011 OI Clarke, Andrew/0000-0003-2293-1423; NR 51 TC 35 Z9 38 U1 0 U2 11 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 MAY PY 2006 VL 23 IS 5 BP 893 EP 900 DI 10.1093/molbev/msj092 PG 8 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 039QH UT WOS:000237320800008 PM 16401685 ER PT J AU Ickert-Bond, SM Wen, J AF Ickert-Bond, SM Wen, J TI Phylogeny and biogeography of Altingiaceae: Evidence from combined analysis of five non-coding chloroplast regions SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE biogeography; phylogeny; altingiaceae; divergence times; Liquidambar; Hamamelidaceae ID ESTIMATING DIVERGENCE TIMES; DNA-SEQUENCE EVOLUTION; NORTH-AMERICAN; LIQUIDAMBAR HAMAMELIDACEAE; MOLECULAR EVOLUTION; MAXIMUM-LIKELIHOOD; INTERSPECIFIC RELATIONSHIPS; MORPHOLOGICAL STASIS; GENETIC-DIVERGENCE; BAYESIAN-INFERENCE AB The Altingiaceae consist of similar to 15 species that are disjunctly distributed in Asia and North America. The genus Liquidambar has been employed as a biogeographic model for studying the Northern Hemisphere intercontinental disjunctions. Parsimony and Bayesian analyses based oil five non-coding chloroplast regions support that (1) Liquidambar is paraphyletic; (2) the temperate Liquidambar acalycina and Liquidambar formosana are nested within a large tropical to Subtropical Asian clade; (3) Semiliquidambar is scattered in the eastern Asian clade and is of hybrid origin involving at least two maternal species: L. formosana and L. acalycina; and (4) the eastern North American Liquidambar styraciflua groups with the western Asian Liquidambar orientalis. but is highly distinct from other lineages. Biogeographically, our results demonstrate the complexity of biogeographic migrations throughout the history of Altingiaceae since the Cretaceous, with migration across both the Bering and the North Atlantic land bridges. (c) 2005 Elsevier Inc. All rights reserved. C1 Field Museum, Dept Bot, Chicago, IL 60605 USA. Smithsonian Inst, Dept Bot, United State Natl Herbarium, Washington, DC 20013 USA. Natl Museum Nat Hist, Washington, DC 20013 USA. Chinese Acad Sci, Inst Bot, Lab Systemat & Evolutionary Bot & Herbarium, Beijing 100093, Peoples R China. RP Ickert-Bond, SM (reprint author), Field Museum, Dept Bot, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. EM sbond@fieldmuseum.org RI Ickert-Bond, Stefanie/B-3216-2012 OI Ickert-Bond, Stefanie/0000-0001-8198-8898 NR 122 TC 35 Z9 38 U1 1 U2 5 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 MAY PY 2006 VL 39 IS 2 BP 512 EP 528 DI 10.1016/j.ympev.2005.12.003 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 037UD UT WOS:000237171900019 PM 16439163 ER PT J AU Ginsburg, I Loeb, A AF Ginsburg, I Loeb, A TI The fate of former companions to hypervelocity stars originating at the Galactic Centre SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; stellar dynamics; Galaxy : centre; Galaxy : kinematics and dynamics ID SAGITTARIUS-A-ASTERISK; BLACK-HOLE; MASS; DYNAMICS; BINARIES; GALAXY AB The hypervelocity star SDSS J090745.0+024507 in the halo of the Milky Way galaxy most likely originated from the breakup of a binary star system by the central black hole, SgrA*. We examine the fate of former binary companions to similar hypervelocity stars (HVSs) by simulating 600 different binary orbits around SgrA* with a direct N-body integration code. For some orbital parameters, the binary breakup process leads to HVSs with ejection velocities that are almost an order of magnitude larger than the velocity observed for SDSS J090745.0+024507. The former companion stars populate highly eccentric orbits which resemble the observed orbits for some of the stars nearest to SgrA*. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ginsburg, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM iginsburg@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 23 TC 53 Z9 53 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2006 VL 368 IS 1 BP 221 EP 225 DI 10.1111/j.1365-2966.2006.10091.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032TM UT WOS:000236797600034 ER PT J AU Hardcastle, MJ Kraft, RP Worrall, DM AF Hardcastle, MJ Kraft, RP Worrall, DM TI The infrared jet in Centaurus A: multiwavelength constraints on emission mechanisms and particle acceleration SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : individual; Centaurus A; galaxies : jets ID X-RAY STRUCTURE; CHANDRA OBSERVATIONS; RADIO-LOBE; NUCLEI; DUST AB We report on Spitzer and Gemini observations of the jet of Centaurus A in the infrared, which we combine with radio, ultraviolet and X-ray data. Spitzer detects jet emission from about 2 arcmin from the nucleus, the emission becoming particularly bright after the jet flare point at similar to 3.4 arcmin. Where X-ray and infrared emission are seen together the broad-band data strongly support a synchrotron origin for the X-rays. The jet flare point is marked by a broad, diffuse region of X-rays which may be associated with a shock: we discuss possible physical mechanisms for this. The infrared jet persists after the flare point region although X-ray emission is absent; it is plausible that here we are seeing the effects of particle acceleration followed by downstream advection with synchrotron losses. Gemini data probe the inner regions of the jet, putting limits on the mid-infrared flux of jet knots. C1 Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM mjh@star.herts.ac.uk RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 26 TC 27 Z9 27 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 MAY 1 PY 2006 VL 368 IS 1 BP L15 EP L19 DI 10.1111/j.1745-3933.2006.00146.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032TM UT WOS:000236797600004 ER PT J AU McKinney, JC AF McKinney, JC TI Relativistic force-free electrodynamic simulations of neutron star magnetospheres SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE relativity; stars : pulsars; general; stars : winds, outflows ID AXISYMMETRICAL PULSAR MAGNETOSPHERE; BLACK-HOLE; EVOLUTION AB The luminosity and structure of neutron star magnetospheres are crucial to our understanding of pulsar and plerion emission. A solution found using the force-free approximation would be an interesting standard with which any model with more physics could be compared. Prior quasi-analytic force-free solutions may not be stable, while prior time-dependent magnetohydrodynamic models used unphysical model parameters. We use a time-dependent relativistic force-free electrodynamics code with no free parameters to find a unique stationary solution for the axisymmetric rotating pulsar magnetosphere in a Minkowski space-time in the case of no surface currents on the star. The solution is similar to the force-free quasi-analytic solution found in 1999 by Contopoulos, Kazanas & Fendt and the numerical magnetohydrodynamic solution found in 2006 by Komissarov. The magnetosphere structure and the usefulness of the classical y-point in the general dissipative regime are discussed. The pulsar luminosity is found to be L approximate to 0.99 +/- 0.01 mu(2)Omega(4)(star)/c(3) for a dipole moment mu and stellar angular frequency Omega(star). C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP McKinney, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM jmckinney@cfa.harvard.edu NR 24 TC 82 Z9 82 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2006 VL 368 IS 1 BP L30 EP L34 DI 10.1111/j.1745-3933.2006.00150.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032TM UT WOS:000236797600007 ER PT J AU Kays, RW AF Kays, RW TI My kingdom for a crown SO NATURAL HISTORY LA English DT Editorial Material C1 New York State Museum & Sci Serv, Albany, NY 12230 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Kays, RW (reprint author), New York State Museum & Sci Serv, Albany, NY 12230 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU NATURAL HISTORY MAGAZINE PI NEW YORK PA 36 WEST 25TH STREET, FIFTH FLOOR, NEW YORK, NY 10010 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD MAY PY 2006 VL 115 IS 4 BP 72 EP 72 PG 1 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 033QI UT WOS:000236863500027 ER PT J AU Chen, GX Kirby, K Brickhouse, NS AF Chen, G. X. Kirby, K. Brickhouse, N. S. TI Dirac R-matrix calculation of electron-impact excitation of Ni XIX SO PHYSICAL REVIEW A LA English DT Article ID X-RAY-SPECTRUM; NEON-LIKE IONS; FE-XVII; LABORATORY MEASUREMENTS; COLLISION STRENGTHS; EMISSION-LINES; DIAGNOSTICS; CHANDRA AB The Dirac R-matrix method is used for solving the relativistic close-coupling equations for the electron impact excitation of Ni XIX. Target states up to the principal quantum number n=5 are included in the calculation. Highly accurate results are obtained in our calculations with the inclusion of resonance effects, channel coupling effects, and fully relativistic effects. We demonstrate that strong resonances appear in the excitation of the highly-charged ion Ni XIX, in particular for intercombination and forbidden transitions. Large differences are found when compared with previous calculations carried out with the distorted wave method. This calculation has direct applications to laboratory measurements and observations of astrophysical x-ray sources. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Chen, GX (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 23 TC 8 Z9 8 U1 0 U2 1 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 MAY PY 2006 VL 73 IS 5 AR 052708 DI 10.1103/PhysRevA.73.052708 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 048LT UT WOS:000237949300073 ER PT J AU Lovelock, CE Ball, MC Choat, B Engelbrecht, BMJ Holbrook, NM Feller, IC AF Lovelock, CE Ball, MC Choat, B Engelbrecht, BMJ Holbrook, NM Feller, IC TI Linking physiological processes with mangrove forest structure: phosphorus deficiency limits canopy development, hydraulic conductivity and photosynthetic carbon gain in dwarf Rhizophora mangle SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Belize; fertilization; leaf area index (LAI); photosynthesis; xylem ID LEAF GAS-EXCHANGE; WATER TRANSPORT; NUTRIENT ENRICHMENT; PONDEROSA PINE; SAP FLUX; CONDUCTANCE; XYLEM; GROWTH; VULNERABILITY; CAVITATION AB Spatial gradients in mangrove tree height in barrier islands of Belize are associated with nutrient deficiency and sustained flooding in the absence of a salinity gradient. While nutrient deficiency is likely to affect many parameters, here we show that addition of phosphorus (P) to dwarf mangroves stimulated increases in diameters of xylem vessels, area of conductive xylem tissue and leaf area index (LAI) of the canopy. These changes in structure were consistent with related changes in function, as addition of P also increased hydraulic conductivity (K-s), stomatal conductance and photosynthetic assimilation rates to the same levels measured in taller trees fringing the seaward margin of the mangrove. Increased xylem vessel size and corresponding enhancements in stern hydraulic conductivity in P fertilized dwarf trees came at the cost of enhanced midday loss of hydraulic conductivity and was associated with decreased assimilation rates in the afternoon. Analysis of trait plasticity identifies hydraulic properties of trees as more plastic than those of leaf structural and physiological characteristics, implying that hydraulic properties are key in controlling growth in mangroves. Alleviation of P deficiency, which released trees from hydraulic limitations, reduced the structural and functional distinctions between dwarf and taller fringing tree forms of Rhizophora mangle. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. Australian Natl Univ, Res Sch Biol Sci, Canberra, ACT 0200, Australia. Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM c.lovelock@uq.edu.au RI Choat, Brendan/C-8445-2009; Ball, Marilyn/D-1180-2009; Engelbrecht, Bettina/E-9914-2012; Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 NR 44 TC 57 Z9 64 U1 6 U2 34 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0140-7791 EI 1365-3040 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD MAY PY 2006 VL 29 IS 5 BP 793 EP 802 DI 10.1111/j.1365-3040.2005.01446.x PG 10 WC Plant Sciences SC Plant Sciences GA 037FS UT WOS:000237133100006 PM 17087463 ER PT J AU Tryon, CA McBrearty, S AF Tryon, CA McBrearty, S TI Tephrostratigraphy of the Bedded Tuff Member (Kapthurin Formation, Kenya) and the nature of archaeological change in the later middle Pleistocene SO QUATERNARY RESEARCH LA English DT Article DE tephrostratigraphy; Acheulian; Middle Stone Age; Acheulian-MSA transition; Kapthurin Formation; Baringo ID MODERN HUMAN-BEHAVIOR; STONE-AGE TRANSITION; MODERN HUMAN ORIGINS; MODERN HUMANS; HUMAN-EVOLUTION; HOMO-SAPIENS; ETHIOPIA; BARINGO; AFRICA; VARIABILITY AB Correlation of volcaniclastic deposits of the Bedded Tuff Member (K4) of the Kapthurin Formation (Kenya) provides the means to assess the nature of archaeological change during the later middle Pleistocene, a time period critical to human evolution but poorly represented at other African localities. Field stratigraphic evidence, and petrographic and electron microprobe geochemical analyses of volcanic glass and phenocrysts, define eight subdivisions of K4 tephra. These include a succession of deposits from a local volcanic source that erupted intermittently, as well as other tuffs likely from different sources outside the Baringo basin. Upper portions of the Bedded Tuff Member date to similar to 235,000 yr. The Bedded Tuff Member is underlain by sediments that include the Grey Tuff, dated to 509,000 +/- 9000 yr. The tephrostratigraphic framework defined here is used to place Acheulian and Middle Stone Age (MSA) archaeological sites in chronological order. Results show the persistence of Acheulian large cutting tool manufacture after the advent of points, considered an MSA artifact type. Two assemblages from the site of Koimilot record the appearance at similar to 200,000-250,000 yr of a variety of Levallois flake production methods, an integral if incompletely understood feature of the MSA, here likely derived from local technological antecedents. Combined evidence from the tools and flake production methods suggest an incremental and mosaic pattern of change in hominin adaptive strategies during the Acheulian-MSA transition. (c) 2006 University of Washington. All rights reserved. C1 George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Natl Museum Nat Hist, Smithsonian Inst, Human Origin Program, Washington, DC 20560 USA. Univ Connecticut, Dept Anthropol, Storrs, CT 06269 USA. RP Tryon, CA (reprint author), George Washington Univ, Dept Anthropol, 2110 G St NW, Washington, DC 20052 USA. EM catryon@gwu.edu; mcbrearty@uconn.edu RI Tryon, Christian/B-1172-2010; OI Tryon, Christian/0000-0002-2354-3273 NR 72 TC 30 Z9 32 U1 0 U2 4 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 MAY PY 2006 VL 65 IS 3 BP 492 EP 507 DI 10.1016/j.yqres.2006.01.008 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 046PG UT WOS:000237822900014 ER PT J AU DeVorkin, DH AF DeVorkin, DH TI Theaters of time and space: American planetariums, 1930-1970 SO SCIENCE EDUCATION LA English DT Book Review 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. NR 1 TC 0 Z9 0 U1 0 U2 0 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 MAY PY 2006 VL 90 IS 3 BP 569 EP 571 DI 10.1002/sce.20144 PG 3 WC Education & Educational Research SC Education & Educational Research GA 038FR UT WOS:000237204800010 ER PT J AU Stoll, C AF Stoll, C TI When slide rules ruled SO SCIENTIFIC AMERICAN LA English DT Article C1 Univ Arizona, Tucson, AZ 85721 USA. Kitt Peak Natl Observ, Tucson, AZ 85726 USA. Harvard Smithsonian Ctr Astrophys, Oakland, CA USA. RP Stoll, C (reprint author), Univ Arizona, Tucson, AZ 85721 USA. NR 2 TC 1 Z9 1 U1 0 U2 1 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD MAY PY 2006 VL 294 IS 5 BP 80 EP 87 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 033YS UT WOS:000236891500034 PM 16708492 ER PT J AU Small, LM AF Small, LM TI The maestro (John Myers) SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAY PY 2006 VL 37 IS 2 BP 12 EP 12 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 036DX UT WOS:000237052300002 ER PT J AU Cirtain, J Martens, PCH Acton, LW Weber, M AF Cirtain, Jonathan Martens, P. C. H. Acton, L. W. Weber, Mark TI The EUV unresolved corona SO SOLAR PHYSICS LA English DT Article ID SOLAR CORONA; TRANSITION-REGION; DENSITY STRUCTURE; TEMPERATURE; LOOPS; TRACE; EXPLORER; LIMB AB The unresolved corona for three active regions (ARs) above the solar limb is investigated. Intensities measured for ions formed above 1 MK are presented as a function of height above the solar surface. The observed decrease in intensity with altitude is found to be best fit by an exponential. Furthermore, this exponential decrease is approximately the decrease in emission expected for a hydrostatic planar geometry atmosphere, where the scale height temperature is dependent on the dynamics of the AR. For two of the ARs analyzed, we have found that the best-fit temperature derived from the exponential fits is consistent with an isothermal hydrostatic unresolved corona. C1 Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cirtain, J (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM jcirtain@head.cfa.harvard.edu; martens@physics.montana.edu; acton@physics.montana.edu; mweber@head.cfa.harvard.edu NR 20 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAY PY 2006 VL 235 IS 1-2 BP 295 EP 316 DI 10.1007/s11207-006-0035-3 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 042CV UT WOS:000237505800017 ER PT J AU Prince, LM Kress, WJ AF Prince, LM Kress, WJ TI Phylogenetic relationships and classification in Marantaceae: insights from plastid DNA sequence data SO TAXON LA English DT Article DE classification; matK; Marantaceae; phylogeny; trnK intron; trnL-F intergenic spacer region ID SERIES COMOSAE MARANTACEAE; MULTIPLE RANGE TESTS; CANNA CANNACEAE; COSTA-RICA; 5 GENERA; ZINGIBERALES; VARIANCES; INFERENCE; SUPPORT; FLOWERS AB The evolutionary distinctiveness and phylogenetic position of Marantaceae within the Zingiberales is strongly supported, yet relatively little phylogenetic research has been conducted on members of Marantaceae. Phylogenetic analyses of plastid DNA sequence data (matK and 3' intergenic spacer region, and the trnL-F intergenic spacer region) for 80 ingroup, taxa, representing 27 genera were conducted under parsimony criteria. Results identify five major clades and support significant realignments in tribal and "group" circumscriptions. Four non-monophyletic genera, Calathea, Marantochloa, Phrynium, and Schumannianthus are identified. Although significant work remains to identify relationships of the major lineages within Marantaceae and to redefine several problematic genera, we propose a working classification that better reflects the inferred evolutionary history of the family. C1 Natl Museum Nat Hist, US Natl Herbarium, Dept Bot, MRC 166,Smithsonian Inst, Washington, DC 20013 USA. RP Prince, LM (reprint author), Rancho Santa Ana Bot Garden, 1500 N Coll Ave, Claremont, CA 91711 USA. EM linda.prince@cgu.edu NR 82 TC 30 Z9 31 U1 0 U2 6 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 MAY PY 2006 VL 55 IS 2 BP 281 EP 296 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 058CP UT WOS:000238642400005 ER PT J AU Clark, JL Herendeen, PS Skog, LE Zimmer, EA AF Clark, JL Herendeen, PS Skog, LE Zimmer, EA TI Phylogenetic relationships and generic boundaries in the Episcieae (Gesneriaceae) inferred from nuclear, chloroplast, and morphological data SO TAXON LA English DT Article DE Alloplectus; Crantzia; Episcieae; Gesneriaceae; Glossoloma; ITS; trnH-psbA ID GENUS COLUMNEA GESNERIACEAE; MAXIMUM-LIKELIHOOD ANALYSES; CLADISTIC-ANALYSIS; NDHF SEQUENCES; GESNERIOIDEAE GESNERIACEAE; TRIBAL RELATIONSHIPS; RIBOSOMAL DNA; DATA SETS; EVOLUTION; CONGRUENCE AB Episcieae is the most diverse tribe of Gesneriaceae, with 22 genera and over 700 species, or roughly 21% of all Gesneriaceae. The tribe is restricted to the Neotropics and is characterized by axillary flowers derived from a pair-flowered cyme inflorescence by reduction, a three-trace trilacunar node with split lateral bundles, superior ovaries, and with most members having a haploid chromosome number of n = 9 [n = 8 in Codonanthe and Nematanthus]. Most traditionally recognized genera in Episcieae are either known to be non-monophyletic or have not been represented adequately in phylogenetic analyses to test their monophyly. This paper presents phylogenetic analyses utilizing two molecular [the internal transcribed, spacer region of 18S-26S nuclear ribosomal DNA (ITS) and the trnH-psbA intergenic spacer for 155 species] and one morphological (99 characters for 120 species) datasets, combined in a total evidence analysis. All traditionally recognized genera of Episcieae except for the monotypic genus Lampadaria are represented. Of the 21 sampled genera in Episcieae, 16 are represented by the generic type species. The genera Glossoloma and Crantzia are segregated from the genus Alloplectus as traditionally recognized. Other genera that are strongly supported as monophyletic include Alsobia, Columnea (with the inclusion of C. dielsii), Corytoplectus, and Episcia. Drymonia is weakly supported and is shown here to be morphologically diverse and in need of further evaluation. Evolution of fruit structure is examined in the context of the phylogenetic results presented here with two previously unreported features that are here referred to as capsules with tardily dehiscent and non-dehiscent endocarps. Three independent origins of resupinate flowers are inferred for Glossoloma, Nematanthus, and Crantzia. Strongly supported clades have centers of diversity in southeastern Brazil (Nematanthus, Codonanthe, Codonanthopsis, and Paradrymonia anisophylla), northern South America (Alloplectus, Drymonia, Columnea, Neomortonia), Central America (Alsobia, Oerstedina, Rufodorsia, Cobananthus), and two clades with diversity in the Guiana Shield [(Paradrymonia, Nautilocalyx, Chrysothemis) and (Lembocarpus, Cremersia, Rhoogeton)]. Neomortonia, a genus of three species, is poorly supported due to conflict among datasets. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Suitland, MD 20746 USA. RP Clark, JL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012,MRC-166, Washington, DC 20013 USA. EM clarkjo@si.edu RI Zimmer, Elizabeth/G-3890-2011 NR 93 TC 32 Z9 48 U1 0 U2 9 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 MAY PY 2006 VL 55 IS 2 BP 313 EP 336 PG 24 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 058CP UT WOS:000238642400007 ER PT J AU Peres, CA Barlow, J Laurance, WF AF Peres, Carlos A. Barlow, Jos Laurance, William F. TI Detecting anthropogenic disturbance in tropical forests SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Editorial Material ID AMAZONIAN FORESTS; CANOPY DAMAGE; FIRE; MANAGEMENT AB Tropical forests are beleaguered by an array of threats driven by different scales of anthropogenic perturbations, which vary in the degree to which they can be detected by remote sensing. The extent of different patterns of cryptic disturbance often far exceeds the total area deforested, as shown by two recent studies on selective logging in Amazonia. Here, we discuss different forms of disturbance in Amazonian forests and question how much of the apparently intact forest in this region remains relatively undisturbed. C1 Univ E Anglia, Sch Environm Sci, Ctr Ecol Evolut & Conservat, Norwich NR4 7TJ, Norfolk, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Peres, CA (reprint author), Univ E Anglia, Sch Environm Sci, Ctr Ecol Evolut & Conservat, Norwich NR4 7TJ, Norfolk, England. EM C.Peres@uea.ac.uk RI Laurance, William/B-2709-2012; Peres, Carlos/B-1276-2013; Barlow, Jos/E-7861-2014 OI Peres, Carlos/0000-0002-1588-8765; NR 22 TC 76 Z9 84 U1 8 U2 37 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD MAY PY 2006 VL 21 IS 5 BP 227 EP 229 DI 10.1016/j.tree.2006.03.007 PG 3 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 049JX UT WOS:000238013500002 PM 16697907 ER PT J AU Wemmer, C Krishnamurthy, V Shrestha, S Hayek, LA Thant, M Nanjappa, KA AF Wemmer, C Krishnamurthy, V Shrestha, S Hayek, LA Thant, M Nanjappa, KA TI Assessment of body condition in Asian elephants (Elephas maximus) SO ZOO BIOLOGY LA English DT Article DE fat; morphology; morphometries; sexual dimorphism ID AGE AB A method of assessing body condition of Asian elephants (Elephas maximus) is presented. The method uses visual assessment to assign numerical scores to six different regions of the body, which are totaled to give a numerical index ranging from 0-11. The relationship between the index and morphometric variables is compared for a sample of 119 juvenile and young adult elephants from southern India, Nepal, and Myanmar. Mean ages of males and females were similar. Mean index of body condition (with standard error [SE]) was 7.3 +/- 0.2 points. No significant correlation was found between index of body condition and age over both sexes (r = 0.01, n = 50). Results were equivalent when sexes were treated separately (females: r = 0.03, n = 24; males: r = 0.01, n = 26). Sexes did not differ in height of the shoulder or body condition in our sample, but there was significant sexual dimorphism in breadth of the zygomatic arch and three measures of subcutaneous fat: girth of neck, thickness of cervical fold, and thickness of anal flap. These three measures were also significantly correlated with each other. Our assessment method should prove a practical tool for ecologic studies, but the relationship of the index to percentage of body fat should be determined using heavy water dilution methodology. C1 Conservat & Res Ctr, Front Royal, VA USA. Salim Ali Ctr Ornithol & Nat Hist, Coimbatore, Tamil Nadu, India. Inst Anim Studies, Albert Einstein Coll Med, Bronx, NY USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Myanmar Timber Enterprise, Minist Foresty, Mandalay, Myanmar. Karnataka Forest Dept, Mysore, Karnataka, India. RP Wemmer, C (reprint author), 6125 Toms Trail, Magalia, CA 95954 USA. EM chindwin@sbcglobal.net RI khan, raja/B-5726-2012; pasuvalingam, visha/B-5717-2012 NR 23 TC 16 Z9 17 U1 3 U2 14 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2006 VL 25 IS 3 BP 187 EP 200 DI 10.1002/zoo.20099 PG 14 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 059AI UT WOS:000238705300004 ER PT J AU Butz, A Bosch, H Camy-Peyret, C Chipperfield, M Dorf, M Dufour, G Grunow, K Jeseck, P Kuhl, S Payan, S Pepin, I Pukite, J Rozanov, A von Savigny, C Sioris, C Wagner, T Weidner, F Pfeilsticker, K AF Butz, A Bosch, H Camy-Peyret, C Chipperfield, M Dorf, M Dufour, G Grunow, K Jeseck, P Kuhl, S Payan, S Pepin, I Pukite, J Rozanov, A von Savigny, C Sioris, C Wagner, T Weidner, F Pfeilsticker, K TI Inter-comparison of stratospheric O-3 and NO2 abundances retrieved from balloon borne direct sun observations and Envisat/SCIAMACHY limb measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ABSORPTION CROSS-SECTIONS; MOLECULAR SPECTROSCOPIC DATABASE; FOURIER-TRANSFORM SPECTROSCOPY; SOLAR ZENITH ANGLES; NITROGEN-OXIDES; NM REGION; TEMPERATURE-DEPENDENCE; SATELLITE MEASUREMENTS; DIFFERENT LATITUDES; PROFILE RETRIEVAL AB Stratospheric O-3 and NO2 abundances measured by different remote sensing instruments are inter-compared: (1) Line-of-sight absorptions and vertical profiles inferred from solar spectra in the ultra-violet (UV), visible and infrared (IR) wavelength ranges measured by the LPMA/DOAS (Limb Profile Monitor of the Atmosphere/Differential Optical Absorption Spectroscopy) balloon payload during balloon ascent/descent and solar occultation are examined with respect to internal consistency. (2) The balloon borne stratospheric profiles of O-3 and NO2 are compared to collocated space-borne skylight limb observations of the Envisat/SCIAMACHY satellite instrument. The trace gas profiles are retrieved from SCIAMACHY spectra using different algorithms developed at the Universities of Bremen and Heidelberg and at the Harvard-Smithsonian Center for Astrophysics. A comparison scheme is used that accounts for the spatial and temporal mismatch as well as differing photochemical conditions between the balloon and satellite borne measurements. It is found that the balloon borne measurements internally agree to within +/- 10% and +/- 20% for O-3 and NO2, respectively, whereas the agreement with the satellite is +/- 20% for both gases in the 20 km. C1 Univ Heidelberg, Inst Umweltphys, D-6900 Heidelberg, Germany. Univ Paris 06, LPMAA, Paris, France. Univ Bremen, Inst Environm Phys, Bremen, Germany. Univ Bremen, Inst Remote Sensing, Bremen, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leeds, Sch Earth & Environm, Inst Atmospher Sci, Leeds, W Yorkshire, England. Free Univ Berlin, Inst Meteorol, D-1000 Berlin, Germany. Latvian State Univ, Inst Atom Phys & Spect, LV-1063 Riga, Latvia. RP Butz, A (reprint author), Univ Heidelberg, Inst Umweltphys, D-6900 Heidelberg, Germany. EM andre.butz@iup.uni-heidelberg.de RI Butz, Andre/A-7024-2013; Chipperfield, Martyn/H-6359-2013; von Savigny, Christian/B-3910-2014; Boesch, Hartmut/G-6021-2012; OI Butz, Andre/0000-0003-0593-1608; Chipperfield, Martyn/0000-0002-6803-4149; Sioris, Christopher/0000-0003-1168-8755 NR 79 TC 23 Z9 23 U1 0 U2 3 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD APR 24 PY 2006 VL 6 BP 1293 EP 1314 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 036EK UT WOS:000237053600004 ER PT J AU Anker, A Poddoubtchenko, D Wehrtmann, IS AF Anker, A Poddoubtchenko, D Wehrtmann, IS TI Leslibetaeus coibita, n. gen., n. sp., a new alpheid shrimp from the Pacific coast of Panama (Crustacea : Decapoda) SO ZOOTAXA LA English DT Article DE Alpheidae; new genus; new species; Panama; eastern Pacific; rocky intertidal ID TROPICAL EASTERN PACIFIC; SNAPPING SHRIMP; CARIDEAN SHRIMP; CALIFORNIA; COLOMBIA; GULF; COLLECTION; ALPHEOPSIS; RECORDS; MEXICO AB A new alpheid shrimp, Leslibetaeus coibita, n. gen., n. sp., is described on the basis of two specimens extracted from crevices in a shale rock on the rocky intertidal shore in the Isla Coiba National Park, Pacific coast of Panama. Leslibetaeus is characterized by absence of rostrum and orbital teeth; eyes being only partially covered by carapace; sixth abdominal somite without articulated plate; first segment of the antennular peduncle without tooth on ventromesial carina; short scaphocerite; tip of third maxilliped with stout spines; and strap-like epipods present on third maxilliped and first to fifth pereiopod; stout symmetrical chelipeds, with carpus distally strongly lobed and bearing two rows of setae mesially, and chela without snapping mechanism; carpus of second pereiopod five-segmented, with second segment distinctly longer than first; ischium and merus of third pereiopod unarmed. The new genus appears to be relatively basal and not closely related to any of the currently described alpheid genera. The finding of this new taxon in a relatively accessible habitat indicates a yet unexplored biological potential of the Isla Coiba National Park. C1 Smithsonian Trop Res Inst, APO, AA 34002 USA. Univ Costa Rica, Escuela Biol, San Jose 2060, Costa Rica. RP Anker, A (reprint author), Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. EM ankera@si.edu; poddoubtchenkod@si.edu; ingowehrtmann@gmx.de NR 45 TC 6 Z9 7 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 24 PY 2006 IS 1183 BP 27 EP 41 PG 15 WC Zoology SC Zoology GA 034ZY UT WOS:000236970600002 ER PT J AU Bull, V Beltran, M Jiggins, CD McMillan, WO Bermingham, E Mallet, J AF Bull, Vanessa Beltran, Margarita Jiggins, Chris D. McMillan, W. Owen Bermingham, Eldredge Mallet, James TI Polyphyly and gene flow between non-sibling Heliconius species SO BMC BIOLOGY LA English DT Article ID MITOCHONDRIAL-DNA SEQUENCES; DROSOPHILA-PSEUDOOBSCURA; PHYLOGENETIC UTILITY; POPULATION-GENETICS; DOPA DECARBOXYLASE; CLADISTIC-ANALYSIS; ANOPHELES-GAMBIAE; MULLERIAN MIMICRY; HYBRID STERILITY; CLOSE RELATIVES AB Background: The view that gene flow between related animal species is rare and evolutionarily unimportant largely antedates sensitive molecular techniques. Here we use DNA sequencing to investigate a pair of morphologically and ecologically divergent, non-sibling butterfly species, Heliconius cydno and H. melpomene (Lepidoptera: Nymphalidae), whose distributions overlap in Central and Northwestern South America. Results: In these taxa, we sequenced 30-45 haplotypes per locus of a mitochondrial region containing the genes for cytochrome oxidase subunits I and II (CoI/CoII), and intron-spanning fragments of three unlinked nuclear loci: triose-phosphate isomerase (Tpi), mannose-6-phosphate isomerase (Mpi) and cubitus interruptus (Ci) genes. A fifth gene, dopa decarboxylase (Ddc) produced sequence data likely to be from different duplicate loci in some of the taxa, and so was excluded. Mitochondrial and Tpi genealogies are consistent with reciprocal monophyly, whereas sympatric populations of the species in Panama share identical or similar Mpi and Ci haplotypes, giving rise to genealogical polyphyly at the species level despite evidence for rapid sequence divergence at these genes between geographic races of H. melpomene. Conclusion: Recent transfer of Mpi haplotypes between species is strongly supported, but there is no evidence for introgression at the other three loci. Our results demonstrate that the boundaries between animal species can remain selectively porous to gene flow long after speciation, and that introgression, even between non-sibling species, can be an important factor in animal evolution. Interspecific gene flow is demonstrated here for the first time in Heliconius and may provide a route for the transfer of switch-gene adaptations for Mullerian mimicry. The results also forcefully demonstrate how reliance on a single locus may give an erroneous picture of the overall genealogical history of speciation and gene flow. C1 UCL, Dept Biol, Galton Lab, London NW1 2HE, England. Smithsonian Trop Res Inst, Balboa, Panama. Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. RP Mallet, J (reprint author), UCL, Dept Biol, Galton Lab, 4 Stephenson Way, London NW1 2HE, England. EM Vanessa.Bull@fss.pnn.police.uk; mbeltran@staffmail.ed.ac.uk; jiggins@staffmail.ed.ac.uk; omcmillan@nescent.org; eb@naos.si.edu; j.mallet@ucl.ac.uk RI Jiggins, Chris/B-9960-2008; mallet, james/B-5114-2008 OI Jiggins, Chris/0000-0002-7809-062X; NR 83 TC 83 Z9 85 U1 1 U2 18 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1741-7007 J9 BMC BIOL JI BMC Biol. PD APR 21 PY 2006 VL 4 AR 11 DI 10.1186/1741-7007-4-11 PG 17 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 055RD UT WOS:000238467100001 PM 16630334 ER PT J AU Kawamura, S Nakamura, T Ando, M Seto, N Tsubono, K Numata, K Takahashi, R Nagano, S Ishikawa, T Musha, M Ueda, K Sato, T Hosokawa, M Agatsuma, K Akutsu, T Aoyanagi, K Arai, K Araya, A Asada, H Aso, Y Chiba, T Ebisuzaki, T Eriguchi, Y Fujimoto, MK Fukushima, M Futamase, T Ganzu, K Harada, T Hashimoto, T Hayama, K Hikida, W Himemoto, Y Hirabayashi, H Hiramatsu, T Ichiki, K Ikegami, T Inoue, KT Ioka, K Ishidoshiro, K Itoh, Y Kamagasako, S Kanda, N Kawashima, N Kirihara, H Kiuchi, K Kobayashi, S Kohri, K Kojima, Y Kokeyama, K Kozai, Y Kudoh, H Kunimori, H Kuroda, K Maeda, K Matsuhara, H Mino, Y Miyakawa, O Miyoki, S Mizusawa, H Morisawa, T Mukohyama, S Naito, I Nakagawa, N Nakamura, K Nakano, H Nishizawa, A Niwa, Y Nozawa, C Ohashi, M Ohishi, N Ohkawa, M Okutomi, A Oohara, K Sago, N Saijo, M Sakagami, M Sakata, S Sasaki, M Sato, S Shibata, M Shinkai, H Somiya, K Sotani, H Sugiyama, N Tagoshi, H Takahashi, T Takahashi, H Takahashi, R Takano, T Tanaka, T Taniguchi, K Taruya, A Tashiro, H Tokunari, M Tsujikawa, S Tsunesada, Y Yamamoto, K Yamazaki, T Yokoyama, J Yoo, CM Yoshida, S Yoshino, T AF Kawamura, Seiji Nakamura, Takashi Ando, Masaki Seto, Naoki Tsubono, Kimio Numata, Kenji Takahashi, Ryuichi Nagano, Shigeo Ishikawa, Takehiko Musha, Mitsuru Ueda, Ken-ichi Sato, Takashi Hosokawa, Mizuhiko Agatsuma, Kazuhiro Akutsu, Tomotada Aoyanagi, Koh-suke Arai, Koji Araya, Akito Asada, Hideki Aso, Yoichi Chiba, Takeshi Ebisuzaki, Toshikazu Eriguchi, Yoshiharu Fujimoto, Masa-Katsu Fukushima, Mitsuhiro Futamase, Toshifumi Ganzu, Katsuhiko Harada, Tomohiro Hashimoto, Tatsuaki Hayama, Kazuhiro Hikida, Wataru Himemoto, Yoshiaki Hirabayashi, Hisashi Hiramatsu, Takashi Ichiki, Kiyotomo Ikegami, Takeshi Inoue, Kaiki T. Ioka, Kunihito Ishidoshiro, Koji Itoh, Yousuke Kamagasako, Shogo Kanda, Nobuyuki Kawashima, Nobuki Kirihara, Hiroyuki Kiuchi, Kenta Kobayashi, Shiho Kohri, Kazunori Kojima, Yasufumi Kokeyama, Keiko Kozai, Yoshihide Kudoh, Hideaki Kunimori, Hiroo Kuroda, Kazuaki Maeda, Kei-ichi Matsuhara, Hideo Mino, Yasushi Miyakawa, Osamu Miyoki, Shinji Mizusawa, Hiromi Morisawa, Toshiyuki Mukohyama, Shinji Naito, Isao Nakagawa, Noriyasu Nakamura, Kouji Nakano, Hiroyuki Nishizawa, Atsushi Niwa, Yoshito Nozawa, Choetsu Ohashi, Masatake Ohishi, Naoko Ohkawa, Masashi Okutomi, Akira Oohara, Kenichi Sago, Norichika Saijo, Motoyuki Sakagami, Masaaki Sakata, Shihori Sasaki, Misao Sato, Shuichi Shibata, Masaru Shinkai, Hisaaki Somiya, Kentaro Sotani, Hajime Sugiyama, Naoshi Tagoshi, Hideyuki Takahashi, Tadayuki Takahashi, Hirotaka Takahashi, Ryutaro Takano, Tadashi Tanaka, Takahiro Taniguchi, Keisuke Taruya, Atsushi Tashiro, Hiroyuki Tokunari, Masao Tsujikawa, Shinji Tsunesada, Yoshiki Yamamoto, Kazuhiro Yamazaki, Toshitaka Yokoyama, Jun'ichi Yoo, Chul-Moon Yoshida, Shijun Yoshino, Taizoh TI The Japanese space gravitational wave antenna - DECIGO SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 6th Edoardo Amaldi Conference on Gravitational Waves CY JUN 20-24, 2005 CL Okinawa, JAPAN SP IUPAP, Okinawa Prefecture, Inoue Fdn Sci, Fdn Promot Astron AB DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational wave antenna. It aims at detecting various kinds of gravitational waves between 1 mHz and 100 Hz frequently enough to open a new window of observation for gravitational wave astronomy. The preconceptual design of DECIGO consists of three drag-free satellites, 1000 km apart from each other, whose relative displacements are measured by a Fabry-Perot Michelson interferometer. We plan to launch DECIGO in 2024 after a long and intense development phase, including two pathfinder missions for verification of required technologies. C1 Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. Kyoto Univ, Grad Sch Sci, Kyoto 6068502, Japan. Univ Tokyo, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan. CALTECH, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tsukuba, Ibaraki 3058505, Japan. Univ Electrocommun, Inst Laser Sci, Chofu, Tokyo 1828585, Japan. Niigata Univ, Fac Engn, Niigata 9502181, Japan. Waseda Univ, Shinjuku Ku, Tokyo 1698555, Japan. Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan. Hirosaki Univ, Fac Sci & Technol, Hirosaki, Aomori 0368560, Japan. Nihon Univ, Coll Humanities & Sci, Setagaya Ku, Tokyo 1568550, Japan. RIKEN, Wako, Saitama 3510198, Japan. Univ Tokyo, Grad Sch Arts & Sci, Meguro Ku, Tokyo 1538902, Japan. Tohoku Univ, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058563, Japan. Kinki Univ, Sch Sci & Engn, Osaka 5778502, Japan. Univ Wisconsin, Milwaukee, WI 53201 USA. Osaka City Univ, Grad Sch Sci, Osaka 5588585, Japan. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead L41 1LD, Merseyside, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hiroshima Univ, Grad Sch Sci, Hiroshima 7398526, Japan. Ochanomizu Univ, Grad Sch Humanities & Sci, Bunkyo Ku, Tokyo 1128610, Japan. Gunma Astron Observ, Gunma 3770702, Japan. Natl Inst Informat & Commun Technol, Bunkyo Ku, Tokyo 1130001, Japan. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. Niigata Univ, Fac Sci, Niigata 9502181, Japan. Kyoto Univ, Fac Intergrated Human Studies, Kyoto 6068501, Japan. Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. Observ Paris, Sect Meudon, F-92195 Meudon, France. INAMORI Fdn, Kyoto 6008411, Japan. Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Tokyo Inst Technol, Grad Sch Sci & Engn, Meguro Ku, Tokyo 1528550, Japan. RP Kawamura, S (reprint author), Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. EM seiji.kawamura@nao.ac.jp RI Chiba, Takeshi/G-3510-2011; Mukohyama, Shinji/A-4401-2011; Taniguchi, Keisuke/G-2694-2011; Takahashi, Ryuichi/F-3362-2013; Nakamura, Kouji/H-6364-2013; ANDO, MASAKI/G-4989-2014; Ebisuzaki, Toshikazu/N-6998-2014; OI Chiba, Takeshi/0000-0002-9737-2569; Nakamura, Kouji/0000-0001-6148-4289; ANDO, MASAKI/0000-0002-8865-9998; Ebisuzaki, Toshikazu/0000-0002-3918-1166; Nishizawa, Atsushi/0000-0003-3562-0990; Nakano, Hiroyuki/0000-0001-7665-0796 NR 4 TC 135 Z9 138 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD APR 21 PY 2006 VL 23 IS 8 SI SI BP S125 EP S131 DI 10.1088/0264-9381/23/8/S17 PG 7 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 046XQ UT WOS:000237844800018 ER PT J AU Reegen, P Kallinger, T Frast, D Gruberbauer, M Huber, D Matthews, JM Punz, D Schraml, S Weiss, WW Kuschnig, R Moffat, AFJ Walker, GAH Guenther, DB Rucinski, SM Sasselov, D AF Reegen, P Kallinger, T Frast, D Gruberbauer, M Huber, D Matthews, JM Punz, D Schraml, S Weiss, WW Kuschnig, R Moffat, AFJ Walker, GAH Guenther, DB Rucinski, SM Sasselov, D TI Reduction of time-resolved space-based CCD photometry developed for MOST Fabry Imaging data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; space vehicles : instruments; techniques : photometric ID ASTEROSEISMOLOGY; SATELLITE; PROPOSAL; MISSION AB The MOST (Microvariability and Oscillations of Stars) satellite obtains ultraprecise photometry from space with high sampling rates and duty cycles. Astronomical photometry or imaging missions in low Earth orbits, like MOST, are especially sensitive to scattered light from Earthshine, and all these missions have a common need to extract target information from voluminous data cubes. They consist of upwards of hundreds of thousands of two-dimensional CCD frames (or subrasters) containing from hundreds to millions of pixels each, where the target information, superposed on background and instrumental effects, is contained only in a subset of pixels (Fabry Images, defocused images, mini-spectra). We describe a novel reduction technique for such data cubes: resolving linear correlations of target and background pixel intensities. This step-wise multiple linear regression removes only those target variations which are also detected in the background. The advantage of regression analysis versus background subtraction is the appropriate scaling, taking into account that the amount of contamination may differ from pixel to pixel. The multivariate solution for all pairs of target/background pixels is minimally invasive of the raw photometry while being very effective in reducing contamination due to, e.g. stray light. The technique is tested and demonstrated with both simulated oscillation signals and real MOST photometry. C1 Univ Vienna, Dept Astron, A-1180 Vienna, Austria. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ Montreal, Mt Megant Observ, Montreal, PQ H3C 3J7, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reegen, P (reprint author), Univ Vienna, Dept Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM reegen@astro.univie.ac.at NR 23 TC 29 Z9 29 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2006 VL 367 IS 4 BP 1417 EP 1431 DI 10.1111/j.1365-2966.2006.10082.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030AV UT WOS:000236606400006 ER PT J AU Hussain, GAJ Prieto, CA Saar, SH Still, M AF Hussain, GAJ Prieto, CA Saar, SH Still, M TI Spot patterns and differential rotation in the eclipsing pre-cataclysmic variable binary, V471 Tau SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : eclipsing; stars : imaging; stars : individual : V471 Tau; stars : late-type; stars : magnetic fields; stars : spots ID HUBBLE-SPACE-TELESCOPE; ORBITAL PERIOD MODULATION; COOL ACTIVE STARS; WHITE-DWARF; AB-DORADUS; CLOSE BINARIES; MAGNETIC TOPOLOGY; MAIN-SEQUENCE; DYNAMO; DISTRIBUTIONS AB We present surface spot maps of the K2V primary star in the pre-cataclysmic variable binary system, V471 Tau. The spot maps show the presence of large high-latitude spots located at the sub-white dwarf longitude region. By tracking the relative movement of spot groups over the course of four nights (eight rotation cycles), we measure the surface differential rotation rate of the system. Our results reveal that the star is rotating rigidly with a surface shear rate, d Omega= 1.6 +/- 6 mrad d(-1). The single active star AB Dor has a similar spectral type, rotation period and activity level as the K star in V471 Tau, but displays much stronger surface shear (46 < d Omega < 58 mrad d(-1)). Our results suggest that tidal locking may inhibit differential rotation; this reduced shear, however, does not affect the overall magnetic activity levels in active K dwarfs. C1 Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. European Space Agcy, Estec, Res & Sci Support Dept, Div Astrophys, Noordwijk, Netherlands. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Hussain, GAJ (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM gajh@st-and.ac.uk; callende@astro.as.utexas.edu; saar@head-cfa.harvard.edu; martin.still@gsfc.nasa.gov NR 68 TC 25 Z9 26 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2006 VL 367 IS 4 BP 1699 EP 1708 DI 10.1111/j.1365-2966.2006.10073.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030AV UT WOS:000236606400032 ER PT J AU McKinney, JC AF McKinney, JC TI General relativistic force-free electrodynamics: a new code and applications to black hole magnetospheres SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; magnetic fields; MHD; methods; numerical; galaxies; jets; gamma-rays; bursts ID AXISYMMETRICAL PULSAR MAGNETOSPHERE; MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETIZED WINDS; ACCRETION DISKS; JETS; RECONNECTION; SCHEME; FLOWS; INSTABILITY; ENERGY AB The force-free limit of magnetohydrodynamics (MHD) is often a reasonable approximation to model black hole and neutron star magnetospheres. We describe a general relativistic force-free (GRFFE) formulation that allows general relativistic magnetohydrodynamic (GRMHD) codes to directly evolve the GRFFE equations of motion. Established, accurate and well-tested conservative GRMHD codes can simply add a new inversion piece of code to their existing code, while continuing to use all the already-developed facilities present in their GRMHD code. We show how to enforce the E.B= 0 constraint and energy conservation, and we introduce a simplified general model of the dissipation of the electric field to enforce the B-2-E-2 > 0 constraint. We also introduce a simplified yet general method to resolve current sheets, without much reconnection, over many dynamical times. This formulation is incorporated into an existing GRMHD code (HARM), which is demonstrated to give accurate and robust GRFFE results for Minkowski and black hole space-times. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP McKinney, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM jmckinney@cfa.harvard.edu NR 54 TC 70 Z9 70 U1 1 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2006 VL 367 IS 4 BP 1797 EP 1807 DI 10.1111/j.1365-2966.2006.10087.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030AV UT WOS:000236606400044 ER PT J AU Rebillot, PF Badran, HM Blaylock, G Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Chow, YC Cogan, P Cui, W Daniel, M Duke, C Falcone, A Fegan, SJ Finley, JP Fortson, LF Gillanders, GH Grube, J Gutierrez, K Gyuk, G Hanna, D Holder, J Horan, D Hughes, SB Kenny, GE Kertzman, M Kieda, D Kildea, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Maier, G Moriarty, P Perkins, J Pohl, M Quinn, J Ragan, K Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Steele, G Swordy, SP Valcarcel, L Vassiliev, VV Wakely, SP Weekes, TC Zweerink, J Aller, M Aller, H Boltwood, P Jung, I Kranich, D Nilsson, K Pasanen, M Sadun, A Sillanpaa, A AF Rebillot, PF Badran, HM Blaylock, G Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Chow, YC Cogan, P Cui, W Daniel, M Duke, C Falcone, A Fegan, SJ Finley, JP Fortson, LF Gillanders, GH Grube, J Gutierrez, K Gyuk, G Hanna, D Holder, J Horan, D Hughes, SB Kenny, GE Kertzman, M Kieda, D Kildea, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Maier, G Moriarty, P Perkins, J Pohl, M Quinn, J Ragan, K Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Steele, G Swordy, SP Valcarcel, L Vassiliev, VV Wakely, SP Weekes, TC Zweerink, J Aller, M Aller, H Boltwood, P Jung, I Kranich, D Nilsson, K Pasanen, M Sadun, A Sillanpaa, A CA VERITAS Collaboration TI Multiwavelength observations of the blazar Markarian 421 in 2002 December and 2003 January SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Mrk 421); galaxies : jets; gamma rays : observations radiation; mechanisms : nonthermal; X-rays : individual (Mrk 421) ID TEV GAMMA-RAYS; ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; SELF-COMPTON MODEL; X-RAY; SPECTRAL EVOLUTION; LAC OBJECTS; STRONG FLARES; CRAB-NEBULA; MKN 501 AB We report on a multiwavelength campaign on the TeV gamma-ray blazar Mrk 421 performed during 2002 December and 2003 January. These target of opportunity observations were initiated by the detection of X-ray and TeV gamma-ray flares with the All Sky Monitor (ASM) on board the Rossi X-Ray Timing Explorer (RXTE) and the 10 m Whipple gamma-ray telescope. The campaign included observational coverage in the radio (University of Michigan Radio Astronomy Observatory), optical (Boltwood, La Palma KVA 0.6 m; WIYN 0.9 m), X-ray (RXTE pointed telescopes), and TeV gamma-ray (Whipple and HEGRA) bands. At TeV energies, the observations revealed several flares at intermediate flux levels, peaking between 1 and 1.5 times the flux from the Crab Nebula. While the time-averaged spectrum can be fitted with a single power law of photon index Gamma = 2.8 from dN gamma/dE proportional to E-Gamma, we find some evidence for spectral variability. Confirming earlier results, the campaign reveals a rather loose correlation between the X-ray and TeV gamma-ray fluxes. In one case, a very strong X-ray flare is not accompanied by a comparable TeV gamma-ray flare. Although the source flux was variable in the optical and radio bands, the sparse sampling of the optical and radio light curves does not allow us to study the correlation properties in detail. We present a simple analysis of the data with a synchrotron self-Compton model, emphasizing that models with very high Doppler factors and low magnetic fields can describe the data. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. Univ Michigan, Ann Arbor, MI 48109 USA. Univ Calif Davis, Davis, CA 95616 USA. Tuorla Observ, FIN-21500 Piikkio, Finland. Univ Colorado, Dept Phys, Denver, CO 80208 USA. Hlth Sci Ctr, Denver, CO 80208 USA. RP Washington Univ, Dept Phys, St Louis, MO 63130 USA. EM rebillot@physics.wustl.edu; krawcz@wuphys.wustl.edu RI Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Lang, Mark/0000-0003-4641-4201 NR 85 TC 37 Z9 37 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 APR 20 PY 2006 VL 641 IS 2 BP 740 EP 751 DI 10.1086/500653 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AV UT WOS:000236819400009 ER PT J AU Kotov, O Vikhlinin, A AF Kotov, O Vikhlinin, A TI Chandra sample of galaxy clusters at z=0.4-0.55: Evolution in the mass-temperature relation SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; surveys; X-rays : galaxies ID XMM-NEWTON OBSERVATIONS; RAY SCALING RELATIONS; RX J1347.5-1145; FRACTION; SPECTRA; GAS AB We present a spatially resolved analysis of the temperature and gas density profiles in six relaxed galaxy clusters at z = 0.4-0.54 using long-exposure Chandra observations. We derive the total cluster masses within the radius r(500), assuming hydrostatic equilibrium but without assuming isothermality of the intracluster gas. Together with a similar study based on the XMM-Newton observations (Kotov & Vikhlinin), we obtained the mass and temperature measurements for 13 galaxy clusters at 0.4 < z < 0.7 spanning a temperature interval of 3 keV < T < 14 keV. The observed evolution of the M-T relation, relative to the low-redshift references from the Chandra sample of Vikhlinin et al., follows M-500/T-3/2 proportional to E(z)(-alpha), where we measure alpha = 1.02 +/- 0.20 and 1.33 +/- 0.20 for the spectroscopic and gas mass-weighted temperatures, respectively. Both values are in agreement with the expected self-similar evolution, alpha = 1. Assuming that the cluster mass for a given temperature indeed evolves self-similarly, the derived slopes, gamma, of the high-redshift M-T relation, E(z)M-500 proportional to T-gamma, are gamma = 1.55 +/- 0.14 for T-spec and gamma = 1.65 +/- 0.15 for T-mg. Our results show that both the shape and evolution of the cluster M-T relation at z similar or equal to 0.5 are close to predictions of the self-similar theory. C1 Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kotov, O (reprint author), Russian Acad Sci, Inst Space Res, 84-32 Profsojuznaya St GSP7, Moscow 117997, Russia. EM kotov@hea.iki.rssi.ru; avikhlinin@cfa.harvard.edu NR 21 TC 21 Z9 21 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2006 VL 641 IS 2 BP 752 EP 755 DI 10.1086/500553 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AV UT WOS:000236819400010 ER PT J AU Kotov, O Trudolyubov, S Vestrand, WT AF Kotov, O Trudolyubov, S Vestrand, WT TI A cluster of galaxies hiding behind M31: XMM-Newton observations of RX J0046.4+4204 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (RX J0046.4+4204); intergalactic medium; X-rays : galaxies : clusters ID X-RAY-CLUSTERS; M-T RELATION; GAS FRACTION; CHANDRA; ROSAT; MASS; SAMPLE AB We report on our serendipitous discovery with the XMM-Newton Observatory of a luminous X-ray-emitting cluster of galaxies that is located behind the Andromeda galaxy (M31). X-ray emission from the cluster was detected previously by ROSAT and cataloged as RX J0046.4+4204, but it was not recognized as a galaxy cluster. The much greater sensitivity of our XMM-Newton observations revealed diffuse X-ray emission that extends at least 50 and has a surface brightness profile that is well fit by the alpha-beta model with beta = 0.70 +/- 0.08, a core radius r(c) = 56" +/- 16", and alpha = 1.54 +/- 0.25. A joint global spectral fit of the EPIC MOS1, MOS2, and pn observations with the Mewe-Kaastra-Liedahl plasma emission model gives a cluster temperature of 5.5 +/- 0.5 keV. The observed spectra also show high significance iron emission lines that yield a measured cluster redshift of z = 0: 290 with 2% accuracy. For a cosmological model with H-0 = 71 km s(-1) Mpc(-1), Omega(M) = 0.3, and Omega(Lambda) = 0.7, we derive a bolometric luminosity of L-X = (8.4 +/- 0.5); 10(44) ergs s(-1). This discovery of a cluster behind M31 demonstrates the utility of X-ray surveys for finding rich clusters of galaxies, even in directions of heavy optical extinction. C1 Los Alamos Natl Lab, NIS 2, Space & Remote Sci Grp, Los Alamos, NM 87545 USA. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA. RP Los Alamos Natl Lab, NIS 2, Space & Remote Sci Grp, Los Alamos, NM 87545 USA. NR 32 TC 4 Z9 4 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 APR 20 PY 2006 VL 641 IS 2 BP 756 EP 762 DI 10.1086/500630 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AV UT WOS:000236819400011 ER PT J AU Georgakakis, A Georgantopoulos, I Akylas, A Zezas, A Tzanavaris, P AF Georgakakis, A Georgantopoulos, I Akylas, A Zezas, A Tzanavaris, P TI X-ray number counts of normal galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE surveys; X-rays : galaxies; X-rays : general ID FIELD-NORTH SURVEY; STAR-FORMING GALAXIES; LUMINOSITY FUNCTION; SPIRAL GALAXIES; HAYSTACK SURVEY; CATALOG; SOUTH; NEEDLES AB We use the number counts of X-ray-selected normal galaxies to explore their evolution by combining the most recent wide-angle shallow and pencil-beam deep samples available. The differential X-ray number counts, dN/dS, for early- and late-type normal galaxies are constructed separately and then compared with the predictions of the local X-ray luminosity function under different evolution scenarios. The dN/dS of early- type galaxies is consistent with no evolution out to z approximate to 0.5. For late-type galaxies, our analysis suggests that it is the sources with an X-ray-to-optical flux ratio log (f(X)/f(opt)) > -2 that are evolving the fastest. Including these systems in the late-type galaxy sample yields evolution of the form approximate to(1 + z)(2.7) out to z approximate to 0.4. On the contrary, late-type sources with log (f(X)/f(opt)) < -2 are consistent with no evolution. This suggests that the log (f(X)/f(opt)) > -2 population comprises the most powerful and fast-evolving starbursts at moderate and high z. We argue that although residual low-luminosity AGN contamination may bias our results toward stronger evolution, this is unlikely to modify our main conclusions. C1 Univ London Imperial Coll Sci & Technol, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. Natl Observ Athens, Inst Astron & Astrophys, GR-15236 Athens, Greece. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Georgakakis, A (reprint author), Univ London Imperial Coll Sci & Technol, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2BZ, England. RI Georgantopoulos, Ioannis/L-3687-2013; Georgakakis, Antonis/K-4457-2013; Akylas, Athanassios/K-4629-2013; Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Georgakakis, Antonis/0000-0002-3514-2442 NR 26 TC 6 Z9 6 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2006 VL 641 IS 2 BP L101 EP L104 DI 10.1086/503742 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033BA UT WOS:000236819900006 ER PT J AU Stark, AA Lee, Y AF Stark, AA Lee, Y TI Giant molecular clouds are more concentrated toward spiral arms than smaller clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : structure; ISM : clouds; ISM : molecules ID STAR-FORMATION; GALAXY; KINEMATICS; HYDROGEN; PLANE AB From our catalog of Milky Way molecular clouds, created using a temperature thresholding algorithm on the Bell Laboratories survey, we have extracted two subsets: (1) clouds that are definitely larger than 105 M,, (CO)-C-13 even if they are at their "near distance" (i.e., giant molecular clouds [GMCs]), and (2) clouds that are definitely smaller than 10(5) M-circle dot, even if they are at their "far distance." The positions and velocities of these clouds are compared to the loci of spiral arms in (l, v)-space. The radial velocity separation of each cloud from the nearest l, v spiral arm is introduced as a "concentration statistic." Almost all of the GMCs are found near spiral arms. The density of smaller clouds is enhanced near spiral arms, but some clouds (similar to 10% of the smaller clouds) are unassociated with any spiral arm. The median velocity separation between a GMC and the nearest spiral arm is 3.4 +/- 0.6 km s(-1), whereas the median separation between smaller clouds and the nearest spiral arm is 5.5 +/- 0.2 km s(-1). These separations in radial velocity are composed partly of the velocity dispersion of the cloud populations and partly of velocity differences due to spatial separations between the clouds and the spiral arms in the Galactic rotation field. A simple estimate indicates that the spatial separation component is relatively unimportant. The data are therefore consistent with the hypothesis that most molecular clouds in the Milky Way are spatially located in the spiral arms and that the velocity dispersion of the GMCs within the arms is less than that of the smaller clouds. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Taeduk Radio Astron Observ, Korea Astron Observ, Taejon 305348, South Korea. RP Stark, AA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM aas@cfa.harvard.edu; yulee@trao.re.kr OI Stark, Antony/0000-0002-2718-9996 NR 25 TC 26 Z9 26 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2006 VL 641 IS 2 BP L113 EP L116 DI 10.1086/504036 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033BA UT WOS:000236819900009 ER PT J AU Watters, TR McGovern, PJ AF Watters, TR McGovern, PJ TI Introduction to special section: The hemispheric dichotomy of Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CRUSTAL DICHOTOMY; TERRESTRIAL PLANETS; PLATE-TECTONICS; GIANT IMPACT; TOPOGRAPHY; EVOLUTION; ORIGIN; CONVECTION; BOUNDARY; GRAVITY AB The hemispheric dichotomy is one the most fundamental and least understood features of Mars. The papers in this special section address aspects of the origin of the crustal dichotomy and the modification and evolution of the dichotomy boundary and the northern lowlands. These studies utilize new data from a variety of instruments on spacecraft operating in Mars orbit and on the surface. This special section is an outgrowth of a two-day workshop held at the Lunar and Planetary Institute in Houston, Texas. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. RP Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu OI McGovern, Patrick/0000-0001-9647-3096 NR 34 TC 0 Z9 0 U1 0 U2 0 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 APR 20 PY 2006 VL 33 IS 8 AR L08S01 DI 10.1029/2006GL025755 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 039LV UT WOS:000237308100004 ER PT J AU Niven, JE AF Niven, JE TI Visual motion: Homing in on small target detectors SO CURRENT BIOLOGY LA English DT Editorial Material ID SMALL OBJECTS; BEHAVIOR; PURSUIT; NEURONS AB Tracking moving targets is essential for animals that pursue prey or conspecifics. Recent studies in male and female hoverflies have described classes of neurons that detect the movements of small targets against a moving background but the mechanisms generating their responses remain unclear. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Niven, JE (reprint author), Smithsonian Trop Res Inst, Roosvelt Ave,Tupper Bldg 401, Balboa, Ancon, Panama. EM nivenj@si.edu RI Niven, Jeremy/A-5883-2011 NR 16 TC 4 Z9 4 U1 0 U2 6 PU CELL PRESS PI CAMBRIDGE PA 1100 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD APR 18 PY 2006 VL 16 IS 8 BP R292 EP R294 DI 10.1016/j.cub.2006.03.044 PG 3 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 036CD UT WOS:000237047600016 PM 16631577 ER PT J AU Capper, A Tibbetts, IR O'Neil, JM Shaw, GR AF Capper, A Tibbetts, IR O'Neil, JM Shaw, GR TI Dietary selectivity for the toxic cyanobacterium Lyngbya majuscula and resultant growth rates in two species of opisthobranch mollusc SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Bursatella leachii; feeding preference and deterrence; Lyngbya majuscula toxins; sea hare; Stylocheilus striatus (formerly longicauda) ID HARE STYLOCHEILUS-LONGICAUDA; FEEDING PREFERENCE EXPERIMENTS; ALGAL SECONDARY METABOLITES; MARINE NATURAL-PRODUCTS; LEACHII-PLEI RANG; SEA HARES; BURSATELLA-LEACHII; DOLABELLA-AURICULARIA; LABORATORY CULTURE; CHEMICAL DEFENSES AB Trophodynamics of blooms of the toxic marine cyanobacterium Lyngkya majuscula were investigated to determine dietary specificity in two putative grazers: the opisthobranch molluscs, Stylocheilus striatus and Bursatella leachii. S. striatus is associated with L. majuscula blooms and is known to sequester L. majuscula metabolites. The dietary specificity and toxicodynamics of B. leachii in relation to L. majuscula is less well documented. In this study we found diet history had no significant effect upon dietary selectivity of S. striatus when offered a range of plant species. However, L. majuscula chemotype may alter S. striatus' selectivity for this cyanobacterium. Daily biomass increases between small and large size groups of both species were recorded in no-choice consumption trials using L. majuscula. Both S. striatus and B. leachii preferentially consumed L. majuscula containing lyngbyatoxin-a. Increase in mass over a 10-day period in B. leachii (915%) was significantly greater than S. striatus (150%), yet S. striatus consumed greater quantities of L. majuscula (g day(-1)) and thus had a lower conversion efficiency (0.038) than B. leachii (0.081) based on sea hare weight per gram of L. majuscula consumed day(-1). Our findings suggest that growth rates and conversion efficiencies may be influenced by sea hare maximum growth potential, acquisition of secondary metabolites or diet type. (C) 2005 Elsevier B.V. All rights reserved. C1 Univ Queensland, Natl Ctr Environm Toxicol, Coopers Plains, Qld 4108, Australia. Univ Maryland, Ctr Environm Sci, Cambridge, MA USA. Univ Queensland, Sch Life Sci, Ctr Marine Studies, Brisbane, Qld 4072, Australia. RP Capper, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM cappcr@sms.si.edu RI Capper, Angela/B-4403-2012; Tibbetts, Ian/K-6191-2013; O'Neil, Judith/F-9024-2013; OI Tibbetts, Ian/0000-0002-1481-238X; O'Neil, Judith/0000-0002-7697-5299; Capper, Angela/0000-0002-4922-0253 NR 43 TC 8 Z9 8 U1 1 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD APR 18 PY 2006 VL 331 IS 2 BP 133 EP 144 DI 10.1016/j.jembe.2005.10.009 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 035CX UT WOS:000236978700002 ER PT J AU Lynnerup, N Frohlich, B Thomsen, JL AF Lynnerup, N Frohlich, B Thomsen, JL TI Assessment of age at death by microscopy: Unbiased quantification of secondary osteons in femoral cross sections SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article; Proceedings Paper CT International IOFOS Symposium on Forensic Odontology/3rd International Conferenc on Reconstruction of Soft Facial Parts CY MAY 17-20, 2006 CL Leuven, BELGIUM SP IOFOS DE age at death; bone microscopy; osteon; stereology; bone remodelling ID CORTICAL BONE; ALGORITHM; FEMUR AB The microscopic method of age at death determination was introduced by Kerley in 1965 [E.R. Kerley, The microscopic determination of age in human bone, Am. J. Phys. Anthropol, 23 (1965) 149-163.]. However, even though the method has been revised several times, there remain some fundamental issues concerning the reliability of the methods. This is because several basic histological features seen in a cross section of a bone have to be quantified according to the method, but the definition, and hence quantification, of these features leaves room for subjectivity. In a previous study we found that some of these features (osteon fragments and Haversian canals) could not be identified reliably. Only secondary osteons could be identified with a low inter and intra observer error. Furthermore, since the histological features are quantified in only parts of an entire bone cross section, the selection of these parts or areas is a potential source of bias. Finally, unless an unbiased method is used for addressing features on the borders of the selected areas, this will also introduce error. These issues have not been addressed specifically in previous studies. In this study, we used the methods of stereology to choose the regions of interest, as well as for dealing with border phenomena, and we only counted secondary osteons. Our results show a statistically significant increase in the median number of osteons per area unit with increasing age at death. However, this was after exclusion of one outlier. This result is probably due to the limited sample size (N = 24). As such, this study is preliminary, but does warrant applying the described techniques to a larger sample. (c) 2006 Elsevier Ireland Ltd. All rights reserved. C1 Univ Copenhagen, Panum Inst, Dept Forens Pathol, Lab Biol Anthropol, DK-2200 Copenhagen N, Denmark. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Univ So Denmark, Inst Forens Med, Odense, Denmark. RP Lynnerup, N (reprint author), Univ Copenhagen, Panum Inst, Dept Forens Pathol, Lab Biol Anthropol, Blegdamsvej 3, DK-2200 Copenhagen N, Denmark. EM n.lynnerup@antrolab.ku.dk NR 29 TC 5 Z9 6 U1 0 U2 3 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD APR 15 PY 2006 VL 159 SU 1 BP S100 EP S103 DI 10.1016/j.forsciint.2006.02.023 PG 4 WC Medicine, Legal SC Legal Medicine GA 043KA UT WOS:000237598700021 PM 16529894 ER PT J AU Riley, S AF Riley, S TI Don't I know you? SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 15 PY 2006 VL 131 IS 7 BP 68 EP 69 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 034CP UT WOS:000236902700049 ER PT J AU Eguchi, H Bruni, R Huang, YH Kim, YH Mocharnuk-Macchia, AN Romaine, S Seidel, GM Sethumadhavan, B Yao, W AF Eguchi, H Bruni, R Huang, YH Kim, YH Mocharnuk-Macchia, AN Romaine, S Seidel, GM Sethumadhavan, B Yao, W TI Properties of vapor-deposited Au : Er films for metallic magnetic calorimeters SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 11th International Workshop on Low-Temperature Detectors CY JUL 31-AUG 05, 2005 CL Univ Tokyo, Tokyo, JAPAN HO Univ Tokyo DE Au : Er films; magnetic microcalorimeter; X-ray detector AB Prototype metallic magnetic calorimeters (MMC), in which the magnetization of Au:Er sensors has been measured using a DC SQUID, have shown excellent energy resolution for soft X-rays. However, the results to date have been obtained with devices assembled by hand, placing a small (similar to 50 mu m diameter), thin disk of the Au: Er alloy within the loop of the SQUID. This is an unacceptable method for fabricating large focal-plane arrays of detectors required for the next generation of X-ray telescopes. We are therefore investigating the properties of vapor-deposited films produced by DC magnetron sputtering using an Au:Er alloy target. The magnetic properties of 5 mu m thick An: Er films have been investigated from room temperature down to 40 mK. The measured magnetization matches theoretical values down to 200 mK. The films have the same Er concentration as in the target material. At lower temperatures there is indication of enhanced magnetic interactions among the Er ions. We are studying the dependence of this interaction on the parameters used in the deposition process. (c) 2005 Elsevier B.V. All rights reserved. C1 Brown Univ, Dept Phys, Providence, RI 02912 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brown Univ, Dept Phys, Providence, RI 02912 USA. EM hiroshi_eguchi@brown.edu NR 4 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 EI 1872-9576 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD APR 15 PY 2006 VL 559 IS 2 BP 439 EP 441 DI 10.1016/j.nima.2005.12.031 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 035BL UT WOS:000236974700035 ER PT J AU Jereb, P Roper, CFE AF Jereb, P Roper, CFE TI Cephalopods of the Indian Ocean. A review. Part I. Inshore squids (Loliginidae) collected during the international Indian Ocean expedition SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Review ID LOLIGO-CHINENSIS CEPHALOPODA; SEPIOTEUTHIS-LESSONIANA; STATOLITH GROWTH; DUVAUCELI DORBIGNY; WATERS; AGE; AUSTRALIA; COAST; PHOTOLOLIGO; GENERATIONS AB Cephalopods collected during the International Indian Ocean Expedition (IIOE; 1959-1965) and preserved at the Smithsonian Institution Oceanographic Sorting Center were analysed. This present work reports on the squids of the Loliginidae. A total of 378 specimens of Loliginids was identified: Loligo chinensis, Loligo duvaucelii, Loligo edulis, Loligo singhalensis, Loligo (?) sumatrensis, Loliolus hardwickei, and Sepioteuthis lessoniana. A systematic description is provided for each species, as well as its geographic distribution. Extensive updated information on the biology and fishery of each species also is discussed. Basic measurements were taken on each specimen and main morphological indices were computed; these were compared with those reported in the literature for each species. Tables provide measurements, morphological indices and comparisons with other studies. Appendices present information on capture sites, measurements and indices of individuals by sex and stage of maturity. C1 Ist Cent Ric Sci & Tecnol Applicata Mare, I-00166 Rome, Italy. Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Jereb, P (reprint author), Ist Cent Ric Sci & Tecnol Applicata Mare, Via Casalotti 300, I-00166 Rome, Italy. EM p.jereb@icram.org; gsquidinc@earthlink.net NR 187 TC 6 Z9 6 U1 1 U2 8 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 APR 12 PY 2006 VL 119 IS 1 BP 91 EP 136 DI 10.2988/0006-324X(2006)119[91:COTIOA]2.0.CO;2 PG 46 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 036BE UT WOS:000237045000010 ER PT J AU Bannikov, AF Tyler, JC AF Bannikov, AF Tyler, JC TI A new species of the genus Aulorhamphus (Gasterosteiformes : Aulorhamphidae) from the Eocene of the Caucasus in southwestern Russia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID PERCIFORMES AB A new species of the aulorhamphid fish genus dagger Aulorhamphus, A. caucasicus, is described from the Middle Eocene of Russia (Kuma Horizon, North Caucasus) based on six imprints (five with counterparts) of diminutive specimens. Aulorhamphus previously has been known only from the Middle Eocene of Italy (Monte Bolca), where it is represented by two species, A. bolcensis and A. capellinii. C1 Russian Acad Sci, Paleontol Inst, Moscow 117997, Russia. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Bannikov, AF (reprint author), Russian Acad Sci, Paleontol Inst, Profsoyuznaya 123, Moscow 117997, Russia. EM aban@paleo.ru; tylerj@si.edu RI Bannikov, Alexander/P-9902-2015 NR 7 TC 2 Z9 2 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 APR 12 PY 2006 VL 119 IS 1 BP 143 EP 149 DI 10.2988/0006-324X(2006)119[143:ANSOTG]2.0.CO;2 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 036BE UT WOS:000237045000012 ER PT J AU Broderick, AE Loeb, A AF Broderick, AE Loeb, A TI Imaging optically-thin hotspots near the black hole horizon of Sgr A* at radio and near-infrared wavelengths SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; polarization; techniques : interferometric; Galaxy : centre; infrared : general; submillimetre ID COVARIANT MAGNETOIONIC THEORY; K-ALPHA LINE; ACCRETION DISKS; GALACTIC-CENTER; SAGITTARIUS-A; RADIATION; POLARIZATION; PARAMETERS; EMISSION; FEATURES AB Submilliarcsecond astrometry and imaging of the black hole Sgr A* at the Galactic Centre may become possible in the near future at infrared and submillimetre wavelengths. Motivated by the observations of short-term infrared and X-ray variability of Sgr A*, in a previous paper, we computed the expected images and light curves, including polarization, associated with a compact emission region orbiting the central black hole. We extend this work, using a more realistic hotspot model and including the effects of opacity in the underlying accretion flow. We find that at infrared wavelengths, the qualitative features identified by our earlier work are present, namely it is possible to extract the black hole mass and spin from spot images and light curves of the observed flux and polarization. At radio wavelengths, disc opacity produces significant departures from the infrared behaviour, but there are still generic signatures of the black hole properties. Detailed comparison of these results with future data can be used to test general relativity and to improve existing models for the accretion flow in the immediate vicinity of the black hole. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 33 TC 102 Z9 101 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2006 VL 367 IS 3 BP 905 EP 916 DI 10.1111/j.1365-2966.2006.10152.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027AQ UT WOS:000236385600004 ER PT J AU Robertson, B Cox, TJ Hernquist, L Franx, M Hopkins, PF Martini, P Springel, V AF Robertson, B Cox, TJ Hernquist, L Franx, M Hopkins, PF Martini, P Springel, V TI The fundamental scaling relations of elliptical galaxies SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : evolution; galaxies : formation ID DIGITAL SKY SURVEY; SMOOTHED PARTICLE HYDRODYNAMICS; CLUSTER CL 1358+62; DYNAMICALLY HOT GALAXIES; MERGING DISK GALAXIES; DARK-MATTER UNIVERSE; MASS-SIZE RELATIONS; N-BODY SIMULATIONS; DEEP-FIELD-NORTH; TO-LIGHT RATIOS AB We examine the fundamental scaling relations of elliptical galaxies formed through mergers. Using hundreds of simulations to judge the impact of progenitor galaxy properties on the properties of merger remnants, we find that gas dissipation provides an important contribution to tilt in the fundamental plane (FP) relation. Dissipationless mergers of disks produce remnants that occupy a plane similar to that delineated by the virial relation. As the gas content of progenitor disk galaxies is increased, the tilt of the resulting FP relation increases and the slope of the Re-M star relation steepens. For gas fractions f(gas) > 30%, the simulated FP scalings (R-e alpha sigma I-1.55(e)-0.82) approach those observed in the K band(R-e alpha sigma:(1.53) I-e(-0.79)). The dissipationless merging of spheroidal galaxies and the remerging of disk galaxy remnants roughly maintain the tilt of the FP occupied by the progenitor ellipticals., Dry merging of spheroidal systems at redshifts z < 1 is then expected to maintain the stellar-mass FP relations imprinted by gas-rich merging during the epoch of rapid spheroid and supermassive black hole growth at redshifts z approximate to 1-3. We estimate that approximate to 40%-100% of the FP tilt induced by structural properties, as opposed to stellar population effects, owes to trends in the central total-to-stellar mass ratio M-total/ M star produced by dissipation. Gas cooling allows for an increase in central stellar phase-space density relative to dissipationless mergers, thereby decreasing the central M-total/M star. Lower mass systems obtain greater phase-space densities than higher mass systems, producing a galaxy mass-dependent central M-total/M star and a corresponding tilt in the FP. We account for these trends in the importance of dissipation with galaxy mass in terms of the inefficient cooling of collisionally heated gas in massive halos and dynamically varying gas consumption timescales in smaller systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM brobertson@cfa.harvard.edu NR 157 TC 226 Z9 226 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 APR 10 PY 2006 VL 641 IS 1 BP 21 EP 40 DI 10.1086/500360 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800002 ER PT J AU Lidz, A Hopkins, PF Cox, TJ Hernquist, L Robertson, B AF Lidz, A Hopkins, PF Cox, TJ Hernquist, L Robertson, B TI The luminosity dependence of quasar clustering SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; cosmology : theory; large-scale structure of universe ID SUPERMASSIVE BLACK-HOLES; DARK-MATTER HALOES; HIGH-REDSHIFT QUASARS; DIGITAL-SKY-SURVEY; GALAXY FORMATION; HOST GALAXIES; STELLAR OBJECTS; PHYSICAL MODEL; EVOLUTION; MERGERS AB We investigate the luminosity dependence of quasar clustering, inspired by numerical simulations of galaxy mergers that incorporate black hole growth. These simulations have motivated a new interpretation of the quasar luminosity function. In this picture, the bright end of the quasar luminosity function consists of quasars radiating nearly at their peak luminosities, while the faint end consists mainly of very similar sources, but at dimmer phases in their evolution. We combine this model with the statistics of dark matter halos that host quasar activity. We find that, since bright and faint quasars are mostly similar sources seen in different evolutionary stages, a broad range in quasar luminosities corresponds to only a narrow range in the masses of quasar host halos. On average, bright and faint quasars reside in similar host halos. Consequently, we argue that quasar clustering should depend only weakly on luminosity. This prediction is in qualitative agreement with recent measurements of the luminosity dependence of the quasar correlation function (Croom et al.) and the galaxy-quasar cross-correlation function (Adelberger & Steidel). Future precision clustering measurements from the Sloan Digital Sky Survey (SDSS) and the Two Degree Field Survey (2dF), spanning a large range in luminosity, should provide a strong test of our model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 60 TC 77 Z9 77 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 APR 10 PY 2006 VL 641 IS 1 BP 41 EP 49 DI 10.1086/500444 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800003 ER PT J AU Ofek, EO Maoz, D Rix, HW Kochanek, CS Falco, EE AF Ofek, EO Maoz, D Rix, HW Kochanek, CS Falco, EE TI Spectroscopic redshifts for seven lens galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : general; quasars : individual (BR I0952-0115, HE 0047-1756; HE 0230-2130, HE 0435-1223, LBQS 1009-025, PMN J0134-0931, PMN J1632-003, Q1017-207, Q1355-2257, SDSS 0924+021, WFI J2033-472) ID ACTIVE GALACTIC NUCLEI; GRAVITATIONAL LENS; LUMINOSITY EVOLUTION; FUNDAMENTAL PLANE; FIELD GALAXIES; DARK-MATTER; LINE REGION; TIME DELAYS; SKY SURVEY; QUASAR AB The use of gravitationally lensed quasars for cosmological applications and as probes of galaxy structure and evolution requires knowledge about the lens redshift, which is unknown for a large fraction of lenses. We report Very Large Telescope observations of 11 lensed quasars, designed to measure the redshifts of their lens galaxies. We successfully determined the redshifts for seven systems, five of which were previously unknown. The securely measured redshifts for the lensing galaxies are: HE 0047-1756 z 0: 408; PMN J0134-0931 z 0: 766; HE 0230-2130 z = 0.522; HE 0435-1223 z = 0.455; SDSS 0924+021 z = 0.393; LBQS 1009-025 z = 0.871; and WFI J2033-472 z = 0.658,all with uncertainties of 0.001. For four additional systems (BRI 0952-0115, Q1017-207, Q1355-2257, and PMN J1632-003) we estimate tentative redshifts based on some features in their spectra. C1 Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ofek, EO (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM eran@wise.tau.ac.il; dani@wise.tau.ac.il NR 45 TC 29 Z9 29 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP 70 EP 77 DI 10.1086/500403 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800005 ER PT J AU Robertson, B Hernquist, L Cox, TJ Di Matteo, T Hopkins, PF Martini, P Springel, V AF Robertson, B Hernquist, L Cox, TJ Di Matteo, T Hopkins, PF Martini, P Springel, V TI The evolution of the M-BH-sigma relation SO ASTROPHYSICAL JOURNAL LA English DT Review DE black hole physics; galaxies : evolution; galaxies : formation ID SUPERMASSIVE BLACK-HOLES; QUASAR LUMINOSITY FUNCTION; ACTIVE GALACTIC NUCLEI; EARLY-TYPE GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; EXTREMELY LARGE TELESCOPE; FIELD ELLIPTIC GALAXIES; DARK-MATTER UNIVERSE; DIGITAL SKY SURVEY; VELOCITY DISPERSION AB We examine the evolution of the black hole mass-stellar velocity dispersion (M-BH-sigma) relation over cosmic time, using simulations of galaxy mergers that include feedback from supermassive black hole growth. For a range in redshifts z = 0-6, we modify the virial mass, gas fraction, interstellar medium equation of state, surface mass density, and concentration of dark matter halos of the merger progenitors to match those expected at various cosmic times. We find that the slope of the M-BH-sigma relation is insensitive to the redshift-dependent properties of merger progenitors and should be roughly constant at redshifts z = 0-6. For the same feedback efficiency that reproduces the observed amplitude of the M-BH-sigma relation at z = 0, there is a weak redshift dependence to the normalization, corresponding to an evolution in the Faber-Jackson relation, which results from an increasing velocity dispersion for a given galactic stellar mass. We develop a formalism to connect redshift evolution in the M-BH-sigma relation to the scatter in the local relation at z = 0. For an assumed model for the accumulation of black holes with different masses over cosmic time, we show that the scatter in the local relation places severe constraints on the redshift evolution of both the normalization and slope of the M-BH-sigma relation. Furthermore, we demonstrate that the cosmic downsizing of the black hole population introduces a black hole mass-dependent dispersion in the M-BH-sigma relation and that the skewness of the distribution about the locally observed M-BH-sigma relation is sensitive to redshift evolution in the normalization and slope. In agreement with existing constraints, our simulations imply that hierarchical structure formation should produce the relation with small intrinsic scatter, as the physical origin of the M-BH-sigma enjoys a remarkable resiliency to the redshift-dependent properties of merger progenitors. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM brobertson@cfa.harvard.edu RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 116 TC 200 Z9 200 U1 0 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 APR 10 PY 2006 VL 641 IS 1 BP 90 EP 102 DI 10.1086/500348 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800007 ER PT J AU Greene, JE Ho, LC AF Greene, JE Ho, LC TI Measuring stellar velocity dispersions in active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : Seyfert ID DIGITAL SKY SURVEY; BLACK-HOLE MASS; BROAD-LINE REGION; CALCIUM INFRARED TRIPLET; CA-II TRIPLET; GALACTIC NUCLEI; EMISSION-LINE; SEYFERT-1 GALAXIES; GLOBULAR-CLUSTERS; HOST GALAXIES AB We present stellar velocity dispersion (sigma(*)) measurements for a significant sample of 40 broad-line (type 1) active galaxies for use in testing the well-known relation black hole mass and stellar velocity dispersion. The objects are selected to contain Ca II triplet, Mg I b triplet, and Ca H+K stellar absorption features in their optical spectra so that we may use them to perform extensive tests of the systematic biases introduced by both template mismatch and contamination from the active galactic nucleus (AGN). We use the Ca II triplet as a benchmark to evaluate the utility of the other spectral regions in the presence of AGN contamination. Broad Fe II emission, extending from similar to 5050 to 5520 angstrom, in combination with narrow coronal emission lines, can seriously bias sigma(*) measurements from the Mg I b region, highlighting the need for extreme caution in its use. However, we argue that at luminosities constituting a moderate fraction of the Eddington limit, when the Fe II lines are both weak and smooth relative to the stellar lines, it is possible to derive meaningful measurements with careful selection of the fitting region. In particular, to avoid the contamination of coronal lines, we advocate the use of the region 5250-5820 angstrom, which is rich in Fe absorption features. At higher AGN contaminations, the Ca H+K region may provide the only recourse for estimating sigma(*). These features are notoriously unreliable, due to a strong dependence on spectral type, a steep local continuum, and large intrinsic broadening. Indeed, we find a strong systematic trend in comparisons of Ca H+K with other spectral regions. Luckily the offset is well described by a simple linear fit as a function of sigma(*), which enables us to remove the bias and thus extract unbiased sigma(*) measurements from this region. We lay the groundwork for an extensive comparison between black hole mass and bulge velocity dispersion in active galaxies, as described in a companion paper by Greene & Ho. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 90 TC 62 Z9 62 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP 117 EP 132 DI 10.1086/500353 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800009 ER PT J AU Desai, V Armus, L Soifer, BT Weedman, DW Higdon, S Bian, C Borys, C Spoon, HWW Charmandaris, V Brand, K Brown, MJI Dey, A Higdon, J Houck, J Jannuzi, BT Le Floc'h, E Ashby, MLN Smith, HA AF Desai, V Armus, L Soifer, BT Weedman, DW Higdon, S Bian, C Borys, C Spoon, HWW Charmandaris, V Brand, K Brown, MJI Dey, A Higdon, J Houck, J Jannuzi, BT Le Floc'h, E Ashby, MLN Smith, HA TI IRS spectra of two ultraluminous infrared galaxies at z=1.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : evolution; galaxies : formation; galaxies : starburst; infrared : galaxies ID SPITZER-SPACE-TELESCOPE; DEEP SUBMILLIMETER SURVEY; ACTIVE GALACTIC NUCLEI; ARRAY CAMERA IRAC; MIDINFRARED SPECTROSCOPY; SPECTROPHOTOMETRIC STANDARDS; STARBURST GALAXY; SPECTROGRAPH IRS; STAR-FORMATION; EVOLUTION AB We present low-resolution (64 < R < 124) mid-infrared (8-38 mu m) spectra of two z approximate to 1:3 ultraluminous infrared galaxies (ULIRGs) with L-8-1000 mu m approximate to 10(13)L circle dot. The spectra were taken with the Infrared Spectrograph(IRS) on board the Spitzer Space Telescope. Both objects were discovered in the NOAO Deep Wide-Field Survey (NDWFS) Bootes field. MIPS J142824.0+352619 is a bright 160 mu m source with a large infrared- to-optical flux density ratio. Previous authors provided evidence for a foreground lens and estimated an amplification of <= 10, although this factor is currently poorly constrained. The 6.2, 7.7, 11.3, and 12.8 mu m polycyclic aromatic hydrocarbon (PAH) emission bands in its IRS spectrum indicate a redshift of z approximate to 1.3. The large equivalent width of the 6.2 mu m PAH feature indicates that at least 50% of the mid-infrared energy is generated in a starburst, an interpretation supported by a large [Ne II]/[Ne III] ratio and a low upper limit on the X-ray luminosity. SST24 J142827.19+354127.71 has the brightest 24 mu m flux (10.55 mJy) among optically faint (R > 20) galaxies in the NDWFS. Its mid- infrared spectrum lacks emission features, but the broad 9.7 mu m silicate absorption band places this source at z approximate to 1.3. Optical spectroscopy confirms a redshift of z = 1:293 +/- 0:001. Given this redshift, SST24 J142827.19+354127.71 has among the largest rest-frame 5 mu m luminosities known. The similarity of its SED to those of known AGN-dominated ULIRGs and its lack of either PAH features or large amounts of cool dust indicate that the mid- infrared emission is dominated by an AGN rather than a starburst. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Space Infrared Telescope Facil Sci Ctr, Pasadena, CA 91125 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. Observ Paris, Chercheur Associe, F-75014 Paris, France. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, Div Phys Math & Astron, Mail Stop 320-47, Pasadena, CA 91125 USA. RI Charmandaris, Vassilis/A-7196-2008; Brown, Michael/B-1181-2015 OI Charmandaris, Vassilis/0000-0002-2688-1956; Brown, Michael/0000-0002-1207-9137 NR 53 TC 25 Z9 25 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 APR 10 PY 2006 VL 641 IS 1 BP 133 EP 139 DI 10.1086/500426 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800010 ER PT J AU Brand, K Brown, MJI Dey, A Jannuzi, BT Kochanek, CS Kenter, AT Fabricant, D Fazio, GG Forman, WR Green, PJ Jones, CJ McNamara, BR Murray, SS Najita, JR Rieke, M Shields, JC Vikhlinin, A AF Brand, K Brown, MJI Dey, A Jannuzi, BT Kochanek, CS Kenter, AT Fabricant, D Fazio, GG Forman, WR Green, PJ Jones, CJ McNamara, BR Murray, SS Najita, JR Rieke, M Shields, JC Vikhlinin, A TI The Chandra XBootes survey. III. Optical and near-infrared counterparts SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; surveys; X-rays : galaxies ID DEEP FIELD-SOUTH; X-RAY SOURCES; DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOGS; MULTIWAVELENGTH PROJECT; LOCKMAN-HOLE; HELLAS2XMM SURVEY; BOOTES-FIELD; NORTH SURVEY AB The XBootes Survey is a 5 ks Chandra survey of the Bootes Field of the NOAO Deep Wide-Field Survey (NDWFS). This survey is unique in that it is the largest (9.3 deg(2)) contiguous region imaged in X-ray with complementary deep optical and near-infrared (near-IR) observations. We present a catalog of the optical counterparts to the 3213 X-ray point sources detected in the XBootes survey. Using a Bayesian identification scheme, we successfully identified optical counterparts for 98% of the X-ray point sources. The optical colors suggest that the optically detected galaxies are a combination of z < 1 massive early-type galaxies and bluer star-forming galaxies whose optical AGN emission is faint or obscured, whereas the majority of the optically detected point sources are likely quasars over a large redshift range. Our large-area, X-ray-bright, optically deep survey enables us to select a large subsample of sources (773) with high X-ray-to-optical flux ratios (fx/fo > 10). These objects are likely high-redshift and/or dust-obscured AGNs. These sources have generally harder X-ray spectra than sources with 0.1 < fx/fo < 10. Of the 73 X-ray sources with no optical counterpart in the NDWFS catalog, 47 are truly optically blank down to R similar to 25.5 ( the average 50% completeness limit of the NDWFS R-band catalogs). These sources are also likely to be high-redshift and/or dust-obscured AGNs. C1 Natl Opt Astron Observ, Tucson, AZ 85726 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. RP Brand, K (reprint author), Natl Opt Astron Observ, POB 26732, Tucson, AZ 85726 USA. EM brand@noao.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 NR 62 TC 54 Z9 54 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP 140 EP 157 DI 10.1086/500312 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800011 ER PT J AU Avalos, M Lizano, S Rodriguez, LF Franco-Hernandez, R Moran, JM AF Avalos, M Lizano, S Rodriguez, LF Franco-Hernandez, R Moran, JM TI Spectra and sizes of hypercompact HII regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; radiative transfer; radio continuum : ISM; stars : formation ID H-II-REGIONS; RADIO-CONTINUUM; YOUNG STARS; MASS-LOSS; WINDS; ENVIRONMENTS; G34.26+0.15; EVOLUTION AB We present the analysis of the spectra and sizes of the hypercompact H II regions G34.26+0.15 A and B. We compare their radio continuum spectra and angular sizes with simple models of spherical ionized regions bounded by an inner and an outer radius, with a power-law electron density profile, n(e)(r) proportional to r(-alpha). The radio continuum spectra and sizes can be reasonably reproduced by both uniform sphere models and shell models with large inner radii of the order of 500 AU. High spatial resolution observations at v > 15 GHz, where the regions are optically thin, could distinguish between the two models. The optically thin radio emission implies, after accounting for dust absorption of ionizing photons, that the ionizing stars of sources A and B have spectral types earlier than main-sequence B1 type. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Avalos, M (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 72-3, Morelia 58089, Michoacan, Mexico. EM m.avalos@astrosmo.unam.mx OI Moran, James/0000-0002-3882-4414 NR 23 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP 406 EP 409 DI 10.1086/500447 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800032 ER PT J AU Kaaret, P Corbel, S Tomsick, JA Lazendic, J Tzioumis, AK Butt, Y Wijnands, R AF Kaaret, P Corbel, S Tomsick, JA Lazendic, J Tzioumis, AK Butt, Y Wijnands, R TI Evolution of the X-ray jets from 4U 1755-33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (4U 1755-33); stars : winds, outflows; X-rays : binaries ID XTE J1550-564; 4U 1755-33; EMISSION; QUIESCENCE; X1755-338; SPECTRUM; GALAXY; MICROQUASARS; H1743-322; SS-433 AB We report on new X-ray observations of the large-scale jets recently discovered in X-rays from the black hole candidate 4U 1755-33. Our observations in 2004 show that the jets found in 2001 are still present in X-rays. However, sensitive radio observations in 2004 failed to detect the jets. We suggest that synchrotron radiation is a viable emission mechanism for the jets and that thermal bremsstrahlung and inverse Compton emission are unlikely on energetic grounds. In the synchrotron interpretation, the production of X-rays requires acceleration of electrons up to similar to 60 TeV, the jet power is similar to 4 x 10(35) ergs s(-1), and the radio nondetection requires a spectral index alpha > -0.65 (S-v proportional to v(alpha)), which is similar to the indexes found in lobes surrounding some other compact objects. We find an upper limit on the flux of 4U 1755-33 in quiescence of 5 x 10(-16) ergs cm(-2) s(-1) in the 0.3-8 keV band. C1 Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Univ Paris 07, CNRS, CEA Saclay, AIM,UMR 7158,Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. EM philip-kaaret@uiowa.edu NR 27 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 APR 10 PY 2006 VL 641 IS 1 BP 410 EP 417 DI 10.1086/500399 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800033 ER PT J AU Adams, FC Proszkow, EM Fatuzzo, M Myers, PC AF Adams, FC Proszkow, EM Fatuzzo, M Myers, PC TI Early evolution of stellar groups and clusters: Environmental effects on forming planetary systems SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : general; planets and satellites : formation; stars : formation ID SINGLE-STAR SCATTERING; GAUSSIAN CLOUD CONDITIONS; FREE-FLOATING PLANETS; ORION NEBULA CLUSTER; HERBIG AE/BE STARS; N-BODY INTEGRATION; M-CIRCLE-DOT; MOLECULAR CLOUDS; MASSIVE STARS; DYNAMICAL EVOLUTION AB This paper studies the dynamical evolution of young groups/clusters, with N = 100-1000 members, from their embedded stage out to ages of similar to 10 Myr. We use N-body simulations to explore how their evolution depends on the system size N and the initial conditions. Motivated by recent observations suggesting that stellar groups begin their evolution with subvirial speeds, this study compares subvirial starting states with virial starting states. Multiple realizations of equivalent cases (100 simulations per initial condition) are used to build up a robust statistical description of these systems, e. g., the probability distribution of closest approaches, the mass profiles, and the probability distribution for the radial location of cluster members. These results provide a framework from which to assess the effects of groups/clusters on the processes of star and planet formation and to study cluster evolution. The distributions of radial positions are used in conjunction with the probability distributions of the expected far-ultraviolet (FUV) luminosities (calculated here as a function of cluster size N) to determine the radiation exposure of circumstellar disks. The distributions of closest approaches are used in conjunction with scattering cross sections (calculated here as a function of stellar mass using similar to 10(5) Monte Carlo scattering experiments) to determine the probability of disruption for newly formed solar systems. We use the nearby cluster NGC 1333 as a test case in this investigation. The main conclusion of this study is that clusters in this size range have only a modest effect on forming planetary systems. The interaction rates are low, so that the typical solar system experiences a single encounter with closest approach distance b similar to 1000 AU. The radiation exposure is also low, with median FUV flux G(0) similar to 900 (1.4 ergs s(-1) cm(-2)), so that photoevaporation of circumstellar disks is only important beyond 30 AU. Given the low interaction rates and modest radiation levels, we suggest that solar system disruption is a rare event in these clusters. C1 Univ Michigan, Michigan Ctr Theoret Phys, Dept Phys, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Xavier Univ, Dept Phys, Cincinnati, OH 45207 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Michigan, Michigan Ctr Theoret Phys, Dept Phys, 2477 Randall Lab,500 E Univ Ave, Ann Arbor, MI 48109 USA. EM fca@umich.edu NR 86 TC 141 Z9 141 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 APR 10 PY 2006 VL 641 IS 1 BP 504 EP 525 DI 10.1086/500393 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800043 ER PT J AU Millan-Gabet, R Monnier, JD Akeson, RL Hartmann, L Berger, JP Tannirkulam, A Melnikov, S Billmeier, R Calvet, N D'Alessio, P Hillenbrand, LA Kuchner, M Traub, WA Tuthill, PG Beichman, C Boden, A Booth, A Colavita, M Creech-Eakman, M Gathright, J Hrynevych, M Koresko, C Le Mignant, D Ligon, R Mennesson, B Neyman, C Sargent, A Shao, M Swain, M Thompson, R Unwin, S van Belle, G Vasisht, G Wizinowich, P AF Millan-Gabet, R Monnier, JD Akeson, RL Hartmann, L Berger, JP Tannirkulam, A Melnikov, S Billmeier, R Calvet, N D'Alessio, P Hillenbrand, LA Kuchner, M Traub, WA Tuthill, PG Beichman, C Boden, A Booth, A Colavita, M Creech-Eakman, M Gathright, J Hrynevych, M Koresko, C Le Mignant, D Ligon, R Mennesson, B Neyman, C Sargent, A Shao, M Swain, M Thompson, R Unwin, S van Belle, G Vasisht, G Wizinowich, P TI Keck interferometer observations of FU Orionis objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; instrumentation : interferometers; planetary systems : protoplanetary disks; stars : formation; stars : individual ( V1057 Cygnus, V1515 Cygnus, Z Canis Majoris); techniques : high angular resolution ID Z-CANIS-MAJORIS; HERBIG AE/BE STARS; YOUNG STELLAR OBJECTS; T-TAURI STARS; PALOMAR TESTBED INTERFEROMETER; CIRCUMSTELLAR STRUCTURE; INFRARED-EMISSION; DISK MODELS; ACCRETION; SPECTROSCOPY AB We present new K-band long-baseline interferometer observations of three young stellar objects of the FU Orionis class, namely, V1057 Cyg, V1515 Cyg, and Z CMa-SE, obtained at the Keck Interferometer during its commissioning science period. The interferometer clearly resolves the source of near-infrared emission in all three objects. Using simple geometric models, we derive size scales (0.5-4.5 AU) for this emission. All three objects appear significantly more resolved than expected from simple models of accretion disks tuned to fit the broadband optical and infrared spectrophotometry. We explore variations in the key parameters that are able to lower the predicted visibility amplitudes to the measured levels and conclude that accretion disks alone do not reproduce the spectral energy distributions and K-band visibilities simultaneously. We conclude that either disk models are inadequate to describe the near-infrared emission or additional source components are needed. We hypothesize that large-scale emission ( tens of AU) in the interferometer field of view is responsible for the surprisingly low visibilities. This emission may arise in scattering by large envelopes believed to surround these objects. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lab Astrophys Grenoble, F-38400 St Martin Dheres, France. Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Princeton Univ, Princeton, NJ 08544 USA. Univ Sydney, Dept Phys, Sydney, NSW 2006, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. RP CALTECH, Michelson Sci Ctr, Mail Stop 100-22, Pasadena, CA 91125 USA. EM rafael@ipac.caltech.edu RI Kuchner, Marc/E-2288-2012 NR 62 TC 28 Z9 28 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 APR 10 PY 2006 VL 641 IS 1 BP 547 EP 555 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800046 ER PT J AU Mackay, DH van Ballegooijen, AA AF Mackay, DH van Ballegooijen, AA TI Models of the large-scale corona. I. Formation, evolution, and liftoff of magnetic flux ropes SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : evolution; Sun : magnetic fields ID FORCE-FREE; MASS EJECTIONS; ACTIVE-REGION; QUIESCENT PROMINENCES; HEMISPHERIC PATTERN; VECTOR MAGNETOGRAMS; FILAMENT FORMATION; SOLAR PROMINENCES; NULL POINTS; FIELDS AB The response of the large-scale coronal magnetic field to transport of magnetic flux in the photosphere is investigated. In order to follow the evolution on long timescales, the coronal plasma velocity is assumed to be proportional to the Lorentz force (magnetofriction), causing the coronal field to evolve through a series of nonlinear force-free states. Magnetofrictional simulations are used to study the formation and evolution of coronal flux ropes, highly sheared and/or twisted fields located above polarity inversion lines on the photosphere. As in our earlier studies, the three-dimensional numerical model includes the effects of the solar differential rotation and small-scale convective flows; the latter are described in terms of surface diffusion. The model is extended to include the effects of coronal magnetic diffusion, which limits the degree of twist of coronal flux ropes, and the solar wind, which opens up the field at large height. The interaction of two bipolar magnetic regions is considered. A key element in the formation of flux ropes is the reconnection of magnetic fields associated with photospheric flux cancellation at the polarity inversion lines. Flux ropes are shown to form both above the external inversion line between bipoles (representing type B filaments) and above the internal inversion line of each bipole in a sigmoid shape. It is found that once a flux rope has formed, the coronal field may diverge from equilibrium with the ejection of the flux rope. After the flux rope is ejected, the coronal field once again relaxes down to an equilibrium. This ability to follow the evolution of the coronal fields through eruptions is essential for future full-Sun simulations in which multiple bipoles are evolved for many months or years. C1 Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 64 TC 120 Z9 121 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP 577 EP 589 DI 10.1086/500425 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800050 ER PT J AU Noble, SC Gammie, CF McKinney, JC Del Zanna, L AF Noble, SC Gammie, CF McKinney, JC Del Zanna, L TI Primitive variable solvers for conservative general relativistic magnetohydrodynamics SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; methods : numerical; MHD ID BLACK-HOLE; SCHEME; DISKS AB Conservative numerical schemes for general relativistic magnetohydrodynamics (GRMHD) require a method for transforming between "conserved" variables such as momentum and energy density and "primitive" variables such as rest-mass density, internal energy, and components of the four-velocity. The forward transformation (primitive to conserved) has a closed-form solution, but the inverse transformation (conserved to primitive) requires the solution of a set of five nonlinear equations. Here we discuss the mathematical properties of the inverse transformation and present six numerical methods for performing the inversion. The first method solves the full set of five nonlinear equations directly using a Newton-Raphson scheme and a guess from the previous time step. The other methods reduce the five nonlinear equations to either one or two nonlinear equations that are solved numerically. Comparisons between the methods are made using a survey over phase space, a two-dimensional explosion problem, and a general relativistic MHD accretion disk simulation. The run time of the methods is also examined. Code implementing the schemes is available with the electronic edition of the article. C1 Univ Illinois, Dept Phys, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, Florence, Italy. RP Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. EM scn@uiuc.edu; gammie@uiuc.edu; jmckinney@cfa.harvard.edu; ldz@arcetri.astro.it RI Del Zanna, Luca/N-5598-2015; OI Del Zanna, Luca/0000-0001-5200-882X; Gammie, Charles /0000-0001-7451-8935 NR 21 TC 91 Z9 91 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 APR 10 PY 2006 VL 641 IS 1 BP 626 EP 637 DI 10.1086/500349 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AH UT WOS:000236817800055 ER PT J AU Bakos, GA Pal, A Latham, DW Noyes, RW Stefanik, RP AF Bakos, GA Pal, A Latham, DW Noyes, RW Stefanik, RP TI A stellar companion in the HD 189733 system with a known transiting extrasolar planet SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; planetary systems; stars : individual (HD 189733, HD 189733B); stars : low-mass, brown dwarfs ID MASS COMPANION; STAR AB We show that the very close-by (19 pc) K0 star HD 189733, already found to be orbited by a transiting giant planet, is the primary of a double star system, with the secondary being a mid-M dwarf with projected separation of about 216 AU from the primary. This conclusion is based on astrometry, proper-motion and radial velocity measurements, spectral type determination, and photometry. We also detect differential proper motion of the secondary. The data appear consistent with the secondary's orbiting the primary in a clockwise orbit, lying nearly in the plane of the sky (i.e., nearly perpendicular to the orbital plane of the transiting planet), and with period of about 3200 years. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Eotvos Lorand Univ, Dept Astron, H-1518 Budapest, Hungary. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu NR 19 TC 47 Z9 47 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 APR 10 PY 2006 VL 641 IS 1 BP L57 EP L60 DI 10.1086/503671 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AK UT WOS:000236818100015 ER PT J AU Greene, JE Ho, LC AF Greene, JE Ho, LC TI The M-BH-sigma(*) relation in local active galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : Seyfert ID BLACK-HOLE MASS; DIGITAL SKY SURVEY; DRIVEN DISK WINDS; LINE REGION SIZES; GALACTIC NUCLEI; VELOCITY DISPERSION; SEYFERT-1 GALAXY; EMISSION-LINE; HOST GALAXIES; QUASARS AB We examine whether active galaxies obey the same relation between black hole mass and stellar velocity dispersion as inactive systems, using the largest published sample of velocity dispersions for active nuclei to date. The combination of 56 original measurements with objects from the literature not only increases the sample from the 15 considered previously to 88 objects but allows us to cover an unprecedented range in both stellar velocity dispersion (30-268 km s(-1)) and black hole mass (10(5)-10(8.6) M-circle dot). In the M-BH-sigma(*) relation of active galaxies, we find a lower zero point than the best-fit relation of Tremaine et al. for inactive galaxies, and an upper limit on the intrinsic scatter of 0.4 dex. There is also evidence of a flatter slope at low black hole masses. We discuss potential contributors to the observed offsets, including variations in the geometry of the broad-line region, evolution in the M-BH-sigma(*) relation, and differential growth between black holes and galaxy bulges. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 123 Z9 125 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2006 VL 641 IS 1 BP L21 EP L24 DI 10.1086/500507 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 033AK UT WOS:000236818100006 ER PT J AU Mlynczak, MG Johnson, DG Latvakoski, H Jucks, K Watson, M Kratz, DP Bingham, G Traub, WA Wellard, SJ Hyde, CR Liu, X AF Mlynczak, MG Johnson, DG Latvakoski, H Jucks, K Watson, M Kratz, DP Bingham, G Traub, WA Wellard, SJ Hyde, CR Liu, X TI First light from the Far-Infrared Spectroscopy of the Troposphere (FIRST) instrument SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MICHELSON INTERFEROMETER; SPECTROMETER; SYSTEM; EARTH; CLOUDS AB We present first light spectra that were measured by the newly-developed Far-Infrared Spectroscopy of the Troposphere ( FIRST) instrument during a high-altitude balloon flight from Ft. Sumner, NM on 7 June 2005. FIRST is a Fourier Transform Spectrometer designed to measure accurately the far-infrared ( 15 to 100 mm; 650 to 100 wavenumbers, cm(-1)) emission spectrum of the Earth and its atmosphere. The flight data successfully demonstrated the FIRST instrument's ability to observe the entire energetically significant infrared emission spectrum ( 50 to 2000 cm(-1)) at high spectral and spatial resolution on a single focal plane in an instrument with one broad spectral bandpass beamsplitter. Comparisons with radiative transfer calculations demonstrate that FIRST accurately observes the very fine spectral structure in the far-infrared. Comparisons also show excellent agreement between the atmospheric window radiance measured by FIRST and by instruments on the NASA Aqua satellite that overflew the FIRST flight. FIRST opens a new window on the spectrum that can be used for studying atmospheric radiation and climate, cirrus clouds, and water vapor in the upper troposphere. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Space Dynam Lab, Logan, UT 84341 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Mlynczak, Martin/K-3396-2012; Johnson, David/F-2376-2015 OI Johnson, David/0000-0003-4399-5653 NR 15 TC 38 Z9 38 U1 1 U2 3 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 APR 4 PY 2006 VL 33 IS 7 AR L07704 DI 10.1029/2005GL025114 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 033VD UT WOS:000236878100002 ER PT J AU Castro-Esau, KL Sanchez-Azofeifa, GA Rivard, B Wright, SJ Quesada, M AF Castro-Esau, KL Sanchez-Azofeifa, GA Rivard, B Wright, SJ Quesada, M TI Variability in leaf optical properties of Mesoamerican trees and the potential for species classification SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE classification; hyperspectral; interspecific; intraspecific; leaf level; Mesoamerica; tropical trees ID SPATIAL-RESOLUTION IMAGERY; EXTREME-SHADE PLANTS; SPECTRAL REFLECTANCE; ELEVATIONAL GRADIENT; HYPERSPECTRAL DATA; TROPICAL FORESTS; ARID VEGETATION; LAND-COVER; DRY FOREST; LEAVES AB Leaf traits and physiological performance govern the amount of light reflected from leaves at visible and infrared wavebands. Information on leaf optical properties of tropical trees is scarce. Here, we examine leaf reflectance of Mesoamerican trees for three applications: (1) to compare the magnitude of within- and between-species variability in leaf reflectance, (2) to determine the potential for species identification based on leaf reflectance, and (3) to test the strength of relationships between leaf traits (chlorophyll content, mesophyll attributes, thickness) and leaf spectral reflectance. Within species, shape and amplitude differences between spectra were compared within single leaves, between leaves of a single tree, and between trees. We also investigated the variation in a species' leaf reflectance across sites and seasons. Using forward feature selection and pattern recognition tools, species classification within a single site and season was successful, while classification between sites or seasons was not. The implications of variability in leaf spectral reflectance were considered in light of potential tree crown classifications from remote airborne or satellite-borne sensors. Species classification is an emerging field with broad applications to tropical biologists and ecologists, including tree demographic studies and habitat diversity assessments. C1 Univ Alberta, Dept Earth & Atmospher Sci, Earth Observat Syst Lab, Edmonton, AB T6G 2E3, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Nacl Autonoma Mexico, Ctr Invest Ecosist, Morelia, Michoacan, Mexico. RP Sanchez-Azofeifa, GA (reprint author), Univ Alberta, Dept Earth & Atmospher Sci, Earth Observat Syst Lab, Edmonton, AB T6G 2E3, Canada. EM arturo.sanchez@ualberta.ca RI 黄, 建荣/B-8070-2011; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 63 TC 67 Z9 77 U1 1 U2 22 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 APR PY 2006 VL 93 IS 4 BP 517 EP 530 DI 10.3732/ajb.93.4.517 PG 14 WC Plant Sciences SC Plant Sciences GA 031TQ UT WOS:000236727400004 PM 21646212 ER PT J AU Kathriarachchi, H Samuel, R Hoffmann, P Mlinarec, J Wurdack, KJ Ralimanana, HN Stuessy, TF Chase, MW AF Kathriarachchi, H Samuel, R Hoffmann, P Mlinarec, J Wurdack, KJ Ralimanana, HN Stuessy, TF Chase, MW TI Phylogenetics of tribe Phyllantheae (Phyllanthaceae; Euphorbiaceae sensu lato) based on nrITS and plastid matK DNA sequence data SO AMERICAN JOURNAL OF BOTANY LA English DT Review DE ITS; matK; molecular phylogenetics; Phyllanthaccae; Phyllantheae; Phyllanthus; systematics ID OBLIGATE POLLINATION MUTUALISM; NUCLEAR RIBOSOMAL DNA; EPICEPHALA-MOTHS GRACILLARIIDAE; CONTINENTAL UNITED-STATES; POLLEN MORPHOLOGY; MOLECULAR PHYLOGENETICS; SPECIES EUPHORBIACEAE; GENUS PHYLLANTHUS; GLOCHIDION; EVOLUTION AB Phylogenetic relationships within tribe Phyllantheae, the largest tribe of the family Phyllanthaceae, were examined with special emphasis on the large genus Phyllanthus. Nuclear ribosomal ITS and plastid matK DNA sequence data for 95 species of tribe Phyllantheae, including representatives of all subgenera of Phyllanthus (except Cyclanthera) and several hitherto unplaced infrageneric groups, were analyzed. Results for ITS and matK are generally concordant, although some species are placed differently in the plastid and ITS trees, indicating that hybridization/paralogy is involved. Results confirm paraphyly of Phyllanthus in its traditional circumscription with embedded Breynia, Glochidion, Reverchonia, and Sauropus. We favor the inclusion of the embedded taxa in Phyllanthus over further generic segregation. Monophyletic Phyllanthus comprises an estimated 1269 species, making it one of the "giant" genera. Phyllanthus maderaspatensis is sister to all other species of Phyllanthus, and the genus appears to be of paleotropical origin. Subgenera Isocladus, Kirganelia, and Phyllanthus are polyphyletic, whereas other subgenera appear to be monophyletic. Monotypic Reverchonia is sister to P. abnormis, arborescent section Emblica to herbaceous Urinaria, free-floating aquatic P. fluitans to the weed P. caroliniensis, and the phyllocladous section Choretropsis to the delicate leafy P. claussenii. The unique branching architecture known as "phyllanthoid branching" found in most Phyllanthus taxa has been lost (and/or has been derived) repeatedly. Taxonomic divisions within Phyllantheae based on similar pollen morphology are confirmed, and related taxa share similar distributions. We recommend recognition of six clades at generic level: Flueggea s.l. (including Richeriella), Lingelsheimia, Margaritaria, Phyllanthus s.l. (including Breynia, Glochidion, Reverchonia, and Sauropus), P. diandrus, and Savia section Heterosavia. C1 Univ Vienna, Inst Bot, Dept Higher Plant Systemat & Evolut, A-1030 Vienna, Austria. Royal Bot Gardens, Herbarium, Richmond TW9 3AB, Surrey, England. Univ Zagreb, Fac Sci, Dept Mol Biol, HR-10000 Zagreb, Croatia. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ Antananarivo, Dept Biol & Ecol Vegetale, Antananarivo 101, Madagascar. Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. RP Samuel, R (reprint author), Univ Vienna, Inst Bot, Dept Higher Plant Systemat & Evolut, Rennweg 14, A-1030 Vienna, Austria. EM mary.rosabella.samuel@univie.ac.at RI Chase, Mark /A-6642-2011 NR 106 TC 56 Z9 68 U1 3 U2 14 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 APR PY 2006 VL 93 IS 4 BP 637 EP 655 DI 10.3732/ajb.93.4.637 PG 19 WC Plant Sciences SC Plant Sciences GA 031TQ UT WOS:000236727400016 PM 21646224 ER PT J AU Harris, TR Monfort, SL AF Harris, TR Monfort, SL TI Mating behavior and endocrine profiles of wild black and white Colobus monkeys (Colobus guereza): Toward an understanding of their life history and mating system SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE Colobus guereza; life history; mating behavior; reproductive endocrinology ID LANGURS PRESBYTIS-ENTELLUS; HANUMAN LANGURS; POPULATION-DYNAMICS; REPRODUCTIVE STATUS; ENZYME-IMMUNOASSAY; SERUM ESTRADIOL; KAKAMEGA-FOREST; URINARY; EXCRETION; OVULATION AB Black and white colobus monkeys (Colobus guereza, "guerezas") show no external signs of estrus, and little is known about their mating behavior or reproductive endocrinology. To learn more about the life history characteristics and mating system of guerezas, we documented the mating behavior and ovarian hormone profiles of 10 cycling, lactating, and pregnant females in a wild population. We studied six groups of guerezas in Kibale National Park, Uganda, and collected ad libitum data on their mating behavior. We collected urine samples every 1.9 +/- 0.2 days from potentially fertile females and quantified conjugated urinary estrogen (E1S) and progesterone (PdG) metabolites using enzyme immunoassay (EIA). Females solicited 50.5% of copulations, and most copulations occurred during the interval starting 5 days before presumptive ovulation and ending 2-3 days later, with the highest copulatory levels occurring close to ovulation. We show that the median ovarian cycle length is 24 days, the median gestation length is similar to 158 days, the length of lactational amenorrhea is at least 7-8 months, and the median interbirth interval for females with surviving infants is similar to 22 months. We also document overlap between females' receptive periods in one-male, two- to three-female groups, which may mean that male transfer into such groups is potentially profitable. C1 Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. Smithsonian Natl Zool Pk, Washington, DC USA. RP Harris, TR (reprint author), Max Planck Inst Evolutionary Anthropol, Dept Primatol, Deutscher Pl 6, D-04103 Leipzig, Germany. EM taraharris1@juno.com NR 46 TC 10 Z9 10 U1 2 U2 27 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 APR PY 2006 VL 68 IS 4 BP 383 EP 396 DI 10.1002/ajp.20232 PG 14 WC Zoology SC Zoology GA 028RC UT WOS:000236504900006 PM 16534807 ER PT J AU Secord, R Gingerich, PD Smith, ME Clyde, WC Wilf, P Singer, BS AF Secord, Ross Gingerich, Philip D. Smith, M. Elliot Clyde, William C. Wilf, Peter Singer, Brad S. TI Geochronology and mammalian biostratigraphy of middle and upper Paleocene continental strata, Bighorn Basin, Wyoming SO AMERICAN JOURNAL OF SCIENCE LA English DT Article ID MAGNETIC POLARITY STRATIGRAPHY; EOCENE ALLUVIAL PALEOSOLS; GREEN RIVER FORMATION; TIME-SCALE; CENTRAL MONTANA; NORTH-AMERICA; NEW-MEXICO; DEPOSITS; PALEOCLIMATOLOGY; CALIBRATION AB The Bighorn Basin of northwestern Wyoming preserves one of the most complete records of middle Paleocene to lower Eocene continental biota. The geochronology of this important interval depends partly on numerical calibration of the geomagnetic polarity time scale (GPTS), but the middle and late Paleocene parts of the GPTS have been poorly constrained radioisotopically. A new volcanic ash from the northern Bighorn Basin provides the first radioisotopic age for upper middle Paleocene strata (upper Selandian) and is an important calibration point for the base of polarity Chron C26n and the Selandian-Thanetian stage boundary in the GPTS. Sanidine from the ash has a weighted mean age of 59.00 +/- 0.30 (2 sigma) Ma, based on twenty-three (40)Ar/(39)Ar bulk laser-fusion analyses. The ash corroborates the revised age estimate for the base of Chron C26n in the most recent geomagnetic polarity time scale (GPTS-04) and confirms that C26n is older than depicted in the 1995 GPTS. We place Paleocene mammalian biozones in the Bighorn Basin into a refined geochronologic framework. These biozones are the primary basis for biostratigraphic correlation of middle and upper Paleocene continental deposits in North America. New paleomagnetic data provide synchronous tie points for correlation among three stratigraphic sections in the northern Bighorn Basin and to the GPTS. Paleomagnetic correlation, study of new fossil material, review of known faunas, and refined stratigraphy enable us to reevaluate several biozones. We define three new zones based on first occurrences of taxa: the Phenacolemur (Ti-4b), Probathyopsis (Ti-5a, revised), and Copecion (Cf-3, revised) zones. The Phenacolemur zone includes some faunas previously placed in the Plesiadapis churchilli and Plesiadapis fodinatus zones (Ti-4 and Ti-5a, respectively). The Probathyopsis zone replaces the P. fodinatus zone and the Copecion zone replaces the Phenacodus-Ectocion acme zone (Cf-3). Seven of the biozones considered here are subdivisions of the Tiffanian landmammal age. The Tiffanian was originally typified by the Mason Pocket fauna in southwestern Colorado, but it is now much better known from faunas in the northern Bighorn Basin. Biostratigraphic evidence and new paleomagnetic data from the Bighorn Basin indicate that Mason Pocket is considerably older than was previously recognized and occurs in Chron C26r, rather than C25r. The geochronologic framework presented here helps to constrain the temporal ranges of species that occur in the middle and late Tiffanian, and it allows the Bighorn Basin record to be better compared to other faunal, floral, and paleoclimate records, both regionally and globally. C1 Smithsonian Inst, Dept Paleobiol, NMNH, Washington, DC 20013 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. Univ New Hampshire, Dept Earth Sci, Durham, NH 03824 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Secord, R (reprint author), Smithsonian Inst, Dept Paleobiol, NMNH, POB 37012,NHB MRC 121, Washington, DC 20013 USA. EM secordr@si.edu RI Gingerich, Philip/A-6903-2008; Singer, Bradley/F-4991-2012; Clyde, William/C-9595-2017 OI Gingerich, Philip/0000-0002-1550-2674; Singer, Bradley/0000-0003-3595-5168; Clyde, William/0000-0001-8814-3409 NR 105 TC 36 Z9 44 U1 0 U2 3 PU AMER JOURNAL SCIENCE PI NEW HAVEN PA YALE UNIV, PO BOX 208109, NEW HAVEN, CT 06520-8109 USA SN 0002-9599 J9 AM J SCI JI Am. J. Sci. PD APR PY 2006 VL 306 IS 4 BP 211 EP 245 DI 10.2475/04.2006.01 PG 35 WC Geosciences, Multidisciplinary SC Geology GA 063WM UT WOS:000239050600001 ER PT J AU Johnson, EA Post, JE AF Johnson, EA Post, JE TI Water in the interlayer region of birnessite: Importance in cation exchange and structural stability SO AMERICAN MINERALOGIST LA English DT Article DE birriessite; electron microscopy; IR spectroscopy; order-disorder; thermodynamics; XRD data ID X-RAY-DIFFRACTION; CRYSTAL-STRUCTURE DETERMINATIONS; SYNTHETIC NA-BIRNESSITE; METAL SORBED BIRNESSITE; STRETCHING FREQUENCIES; ELECTRON-DIFFRACTION; HEXAGONAL BIRNESSITE; SILICATE-GLASSES; LONE-PAIR; MANGANESE AB Birnessite is an important scavenger of trace metals in soils and aqueous environments. The basic birnessite-type structure consists of sheets of Mn octahedra separated by similar to 7 or similar to 10 angstrom ("buserite") interlayer regions filled with cations and water. Synthetic birnessite-like structures were produced through cation exchange reactions with synthetic Na-birnessite. The unheated, synthetic Mg2+, Ca2+, and Ni2+ layer structures have an similar to 10 angstrom interlayer spacing, whereas the other cation-exchanged synthetic birnessites and the related mineral chalcophanite have an interlayer spacing of similar to 7 angstrom. The Li+, Na+, K+, Cs+, and Pb2+ synthetic birnessites each contain two to three structurally different water sites, as evidenced by Multiple H2O bending and stretching modes in the infrared spectra. The complexity of the water bands in these spectra is likely related to disordering of cations on the interlayer sites. H-birnessite contains structural water and either hydroxyl, hydronium, (H3O+), or both. The small difference in the width of the water stretching modes between room temperature and -180 degrees C indicates that the water molecules in birnessite-like structures are predominantly structurally, rather than dynamically, disordered. Most of the synthetic birnessites, includiing Na- and K-birnessite, undergo significant water loss at temperatures below 100 degrees C. There is a linear relationship between the temperature at which most of the water is lost from a given cation-exchanged birnessite and the heat of hydration of the interlayer cation. This finding implies that the interlayer water is strongly bound to the interlayer cations, and plays an important role in the thermal stability of birnessite-like structures. C1 Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Johnson, EA (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, MRC 0119, Washington, DC 20560 USA. EM johnsoel@ucla.edu NR 42 TC 30 Z9 31 U1 2 U2 33 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD APR PY 2006 VL 91 IS 4 BP 609 EP 618 DI 10.2138/am.2006.2090 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 036RP UT WOS:000237093000016 ER PT J AU Liu, X Chance, K Sioris, CE Newchurch, MJ Kurosu, TP AF Liu, X Chance, K Sioris, CE Newchurch, MJ Kurosu, TP TI Tropospheric ozone profiles from a ground-based ultraviolet spectrometer: a new retrieval method SO APPLIED OPTICS LA English DT Article ID ABSORPTION-MEASUREMENTS; VISIBLE SPECTROMETER; INFORMATION; NO2; DISTRIBUTIONS; POLARIZATION; VALIDATION; DERIVATION; ALGORITHM AB We present, to the best of our knowledge, a new method to retrieve tropospheric ozone (O-3) profiles from ground-based ultraviolet spectroscopic measurements. This method utilizes radiance spectra in the Huggins bands (i.e., 300-340 nm) measured at three off-axis angles (e.g., 45 degrees, 75 degrees, and 85 degrees) normalized to direct-Sun irradiances or zenith-sky radiances with the total column O-3 derived from direct-Sun or zenith-sky measurements as a constraint. The vertical resolution of the retrieved O-3 values ranges from similar to 3 km near the surface to similar to 12 km at 20 km altitude. This method can be used to measure diurnal variation of tropospheric O-3 profiles and is complementary to the Umkehr method that mainly measures ozone profiles in the stratosphere. (c) 2006 Optical Society of America. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. RP Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM xliu@cfa.harvard.edu RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577; Sioris, Christopher/0000-0003-1168-8755 NR 35 TC 4 Z9 4 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD APR 1 PY 2006 VL 45 IS 10 BP 2352 EP 2359 DI 10.1364/AO.45.002352 PG 8 WC Optics SC Optics GA 029OE UT WOS:000236572000028 PM 16608004 ER PT J AU Kewley, LJ Geller, MJ Barton, EJ AF Kewley, LJ Geller, MJ Barton, EJ TI Metallicity and nuclear star formation in nearby galaxy pairs: Evidence for tidally induced gas flows SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : abundances; galaxies : fundamental parameters; galaxies : high-redshift; galaxies : starburst ID CFA REDSHIFT SURVEY; DIGITAL SKY SURVEY; H-II REGIONS; EMISSION-LINE SPECTRA; RICH HII-REGIONS; SPIRAL GALAXIES; MERGING GALAXIES; ABUNDANCE GRADIENTS; CHEMICAL EVOLUTION; INFRARED GALAXIES AB We derive the first luminosity-metallicity (L-Z) relation for a large objectively selected sample of local galaxy pairs, and we compare the L-Z relation of the pairs with the relation for the Nearby Field Galaxy Survey. Galaxy pair members with small projected separations (s < 20 kpc h(-1)) have systematically lower metallicities (similar to 0.2 dex on average) than either the field galaxies or more widely separated pairs at the same luminosity. There is a strong correlation between metallicity and central burst strength in the galaxy pairs. All five galaxies in the pairs sample with strong central bursts have close companions and metallicities lower than the comparable field galaxies. Our results provide strong observational evidence for a merger scenario in which galaxy interactions cause gas flows toward the central regions, carrying less enriched gas from the outskirts of the galaxy into the central regions. The less enriched gas dilutes the preexisting nuclear gas to produce a lower metallicity than would be obtained prior to the interaction. These gas flows trigger central bursts of star formation, causing strong central burst strengths and possibly aiding the formation of blue bulges. We show that the timescale and central gas dilution required by this scenario are consistent with predictions from hydrodynamic merger models. C1 Univ Hawaii, Honolulu, HI 96822 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Kewley, LJ (reprint author), Univ Hawaii, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM kewley@ifa.hawaii.edu NR 131 TC 114 Z9 115 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2004 EP 2017 DI 10.1086/500295 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200011 ER PT J AU Humphreys, RM Jones, TJ Polomski, E Koppelman, M Helton, A McQuinn, K Gehrz, RD Woodward, CE Wagner, RM Gordon, K Hinz, J Willner, SP AF Humphreys, RM Jones, TJ Polomski, E Koppelman, M Helton, A McQuinn, K Gehrz, RD Woodward, CE Wagner, RM Gordon, K Hinz, J Willner, SP TI M33's Variable A: A hypergiant star more than 35 years in eruption SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : individual (M33 Var A); stars : winds, outflows; supergiants ID HUBBLE-SANDAGE VARIABLES; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; VY-CANIS-MAJORIS; RHO-CASSIOPEIAE; COOL HYPERGIANT; HIGH-RESOLUTION; SILICATE DUST; SPECTROSCOPY; SPECTRA AB Variable A in M33 is a member of a rare class of highly luminous, evolved stars near the upper luminosity boundary that show sudden and dramatic shifts in apparent temperature due to the formation of optically thick winds in high mass loss episodes. Recent optical and infrared spectroscopy and imaging reveal that its "eruption," begun in similar to 1950, has ended, having lasted approximate to 45 yr. Our current observations show major changes in its wind from a cool, dense envelope to a much warmer state surrounded by low-density gas with rare emission lines of Ca II, [Ca II], and K I. Its spectral energy distribution has unexpectedly changed, especially at the long wavelengths, with a significant decrease in its apparent flux, while the star remains optically obscured. We conclude that much of its radiation is now escaping out of our line of sight. We attribute this to the changing structure and distribution of its circumstellar ejecta, corresponding to the altered state of its wind as the star recovers from a high mass loss event. C1 Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Humphreys, RM (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM roberta@aps.umn.edu NR 37 TC 27 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2105 EP 2113 DI 10.1086/500811 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200019 ER PT J AU Struble, MF Galatola, A Faccioli, L Alcock, C Cruz, K AF Struble, MF Galatola, A Faccioli, L Alcock, C Cruz, K TI Evidence for companion-induced secular changes in the turbulent disk of a be star in the large magellanic cloud MACHO database SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : emission-line, Be; stars : variables : other ID GRAVITATIONAL LENSING EXPERIMENT; KH 15D; CIRCUMSTELLAR DISK; VARIABLE-STARS; PROTOPLANETARY DISKS; STELLAR COMPANIONS; ACCRETION DISCS; DUST DISK; BINARY; ECLIPSES AB The light curve of a blue variable in the MACHO LMC database (FTS ID78.5979.72) appeared nearly unvarying for about 4 yr (the quasi-flat segment) but then rapidly changed to become periodic with noisy minima for the remaining 4 yr ( the periodic segment); there are no antecedent indications of a gradual approach to this change. Lomb periodogram analyses indicate the presence of two distinct periods of similar to 61 and 8 days in both the quasi-flat and the periodic segments. Minima of the periodic segment cover at least 50% of the orbital period and contain spikes of light with the 8 day period; maxima do not show this short period. The system typically shows maxima to be redder than minima. The most recent OGLE-III light curve shows only a 30 day periodicity. The variable's Vand R magnitudes and color are those of a Be star, and recent sets of near-infrared spectra 4 days apart, secured during the time of the OGLE-III data, show H alpha emission near and at a maximum, confirming its Be star characteristics. The model that best fits the photometric behavior consists of a thin ringlike circumstellar disk of low mass with four obscuring sectors orbiting the central B star in unison at the 61 day period. The central star peers through the three equispaced separations between the four sectors producing the 8 day period. These sectors could be dusty vortices comprised of particles larger than typical interstellar dust grains that dim but selectively scatter the central star's light, while the remainder of the disk contains hydrogen in emission, making maxima appear redder. A companion star of lower mass in an inclined and highly eccentric orbit produces an impulsive perturbation near its periastron to change the disk's orientation, changing eclipses from partial to complete within similar to 10 days. The most recent change to a 30 day period observed in the OGLE-III data may be caused by obscuring sectors that have coalesced into larger ones and spread out along the disk. C1 Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. RP Struble, MF (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM struble@physics.upenn.edu; agalatola@wcupa.edu; lfaccioli@lbl.gov; calcock@cfa.harvard.edu; kelle@amnh.org OI Cruz, Kelle/0000-0002-1821-0650 NR 61 TC 2 Z9 2 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 APR PY 2006 VL 131 IS 4 BP 2196 EP 2208 DI 10.1086/500806 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200024 ER PT J AU Sozzetti, A Yong, D Carney, BW Laird, JB Latham, DW Torres, G AF Sozzetti, A Yong, D Carney, BW Laird, JB Latham, DW Torres, G TI Chemical composition of the planet-harboring star TrES-1 SO ASTRONOMICAL JOURNAL LA English DT Review DE planetary systems; solar neighborhood; stars : abundances; stars : individual (GSC 02652-01324); stars : kinematics ID RELATIVE OSCILLATOR-STRENGTHS; GALACTIC THICK DISK; EXTRA-SOLAR PLANETS; METAL-RICH STARS; LY-ALPHA SYSTEMS; HOST STARS; PARENT STARS; GIANT PLANETS; STELLAR METALLICITY; DWARF STARS AB We present a detailed chemical abundance analysis of the parent star of the transiting extrasolar planet TrES-1. Based on high-resolution Keck HIRES and Hobby-Eberly Telescope HRS spectra, we have determined abundances relative to the Sun for 16 elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Y, and Ba). The resulting average abundance of <[X/H]> = - 0.02 +/- 0.06 is in good agreement with initial estimates of solar metallicity based on iron. We compare the elemental abundances of TrES-1 with those of the sample of stars with planets, searching for possible chemical abundance anomalies. TrES-1 appears not to be chemically peculiar in any measurable way. We investigate possible signs of selective accretion of refractory elements in TrES-1 and other stars with planets and find no statistically significant trends of metallicity [X/H] with condensation temperature T-c. We use published abundances and kinematic information for the sample of planet-hosting stars ( including TrES-1) and several statistical indicators to provide an updated classification in terms of their likelihood to belong to either the thin disk or the thick disk of the Milky Way. TrES-1 is found to be very likely a member of the thin-disk population. By comparing alpha-element abundances of planet hosts and a large control sample of field stars, we also find that metal-rich ([Fe/H] greater than or similar to 0.0) stars with planets appear to be systematically underabundant in [alpha/Fe] by approximate to 0.1 dex with respect to comparison field stars. The reason for this signature is unclear, but systematic differences in the analysis procedures adopted by different groups cannot be ruled out. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. RP Sozzetti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asozzett@cfa.harvard.edu; yong@physics.unc.edu; bruce@physics.unc.edu; laird@tycho.bgsu.edu; dlatham@cfa.harvard.edu; gtorres@cfa.harvard.edu OI Sozzetti, Alessandro/0000-0002-7504-365X NR 123 TC 18 Z9 18 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2274 EP 2289 DI 10.1086/500639 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200031 ER PT J AU Raman, A Lisanti, M Wilner, DJ Qi, C Hogerheijde, M AF Raman, A Lisanti, M Wilner, DJ Qi, C Hogerheijde, M TI A Keplerian disk around the herbig Ae star HD 169142 SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems : protoplanetary disks; stars : individual (HD 169142); stars : pre-main-sequence ID INTERMEDIATE-MASS STARS; CIRCUMSTELLAR DISKS; HIGH-RESOLUTION; ACCRETION DISKS; AE/BE SYSTEMS; T-TAURI; DUST; GAS; SPECTROSCOPY; EMISSION AB We present Submillimeter Array observations of the Herbig Ae star HD 169142 in 1.3 mm continuum emission and (CO)-C-12 J = 2-1 line emission at similar to 1."5 resolution that reveal a circumstellar disk. The continuum emission is centered on the star position and resolved, and it provides a mass estimate of similar to 0.02 M-circle dot for the disk. The CO images show patterns in position and velocity that are well matched by a disk in Keplerian rotation with low inclination to the line of sight. We use radiative transfer calculations based on a flared, passive disk model to constrain the disk parameters by comparison to the spectral line emission. The derived disk radius is 235 AU, and the inclination is 13 degrees. The model also necessitates modest depletion of the CO molecules, similar to that found in Keplerian disks around T Tauri stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Raman, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Raman, Aaswath/H-4245-2013 OI Raman, Aaswath/0000-0003-0106-8341 NR 27 TC 26 Z9 26 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2290 EP 2293 DI 10.1086/500587 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200032 ER PT J AU Mamajek, EE Meyer, MR Liebert, J AF Mamajek, EE Meyer, MR Liebert, J TI Post-T tauri stars in the nearest OB association (vol 124, pg 1670, 2002) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ USA. RP Mamajek, EE (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 13 Z9 13 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2360 EP 2360 DI 10.1086/501012 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200038 ER PT J AU Bernstein, GM Trilling, DE Allen, RL Brown, ME Holman, M Malhotra, R AF Bernstein, GM Trilling, DE Allen, RL Brown, ME Holman, M Malhotra, R TI The size distribution of trans-neptunian bodies (vol 128, pg 1364, 2004) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Bernstein, GM (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM garyb@physics.upenn.edu; trilling@astro.upenn.edu; lallen@astro.ubc.ca; mbrown@gps.caltech.edu; mholman@cfa.harvard.edu; renu@lpl.arizona.edu NR 1 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2006 VL 131 IS 4 BP 2364 EP 2364 DI 10.1086/503194 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026SA UT WOS:000236361200041 ER PT J AU Wehrse, R Kalkofen, W AF Wehrse, R Kalkofen, W TI Advances in radiative transfer SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Article DE radiative transfer; methods of solution for transfer equation; specific intensity; polarization; many lines ID MOVING-MEDIA; TRANSFER EQUATION; FINITE-ELEMENTS; SPECTRAL-LINES; OPACITY; DIFFUSION; APPROXIMATION; HYDRODYNAMICS; SLAB AB This review describes advances in radiative transfer theory since about 1985. We stress fundamental aspects and emphasize modern methods for the numerical Solution of the transfer equation for spatially multidimensional problems, for both unpolarized and polarized radiation. We restrict the discussion to two level atoms with noninverted populations for given temperature, density and velocity fields. C1 Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. Univ Heidelberg, Interdisziplinares Zentrum Wissensch Rechnen, D-69120 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wehrse, R (reprint author), Univ Heidelberg, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. EM wehrse@ita.uni-heidelberg.de; wolf@cfa.harvard.edu NR 71 TC 6 Z9 6 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0935-4956 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD APR PY 2006 VL 13 IS 1-2 BP 3 EP 29 DI 10.1007/s00159-006-0029-z PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038TG UT WOS:000237251800001 ER PT J AU Kohl, JL Noci, G Cramner, SR Raymond, JC AF Kohl, JL Noci, G Cramner, SR Raymond, JC TI Ultraviolet spectroscopy of the extended solar corona SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE solar wind; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation; techniques : spectroscopic; telescopes ID ION-CYCLOTRON WAVES; KINETIC ALFVEN WAVES; INTERPLANETARY MAGNETIC-FIELD; WIND ACCELERATION REGION; WHITE-LIGHT IMAGES; WHOLE SUN MONTH; R-CIRCLE-DOT; ANISOTROPIC VELOCITY DISTRIBUTIONS; ANGLE SPECTROMETRIC CORONAGRAPH; KELVIN-HELMHOLTZ INSTABILITIES AB The first observations of ultraviolet spectral line profiles and intensities from the extended solar corona (i.e., more than 1.5 solar radii from Sun-center) were obtained oil 13 April 1979 when a rocket-borne ultraviolet coronagraph spectrometer of the Harvard-Smithsonian Center for Astrophysics made direct measurements of proton kinetic temperatures, and obtained upper limits Oil Outflow velocities in a quiet coronal region and a polar coronal hole. Following those observations, ultraviolet coronagraphic spectroscopy has expanded to include observations of over 60 spectral lines in coronal holes, streamers, coronal jets, and solar flare/coronal mass ejection (CME) events. Spectroscopic diagnostic techniques have been developed to determine proton, electron and ion kinetic temperatures and velocity distributions, proton and ion bulk flow speeds and chemical abundances. The observations have been made during three sounding rocket flights, four Shuttle deployed and retrieved Spartan 201 flights, and the Solar and Heliospheric Observatory (SOHO) mission. Ultraviolet spectroscopy of the extended solar corona has led to fundamentally new views of the acceleration regions of the solar wind and CMEs. Observations with the Ultraviolet Coronagraph Spectrometer (UVCS) oil SOHO revealed surprisingly large temperatures, outflow speeds, and velocity distribution anisotropies in coronal holes, especially for minor ions. Those measurements have guided theorists to discard some candidate physical processes of solar wind acceleration and to increase and expand investigations of ion cyclotron resonance and related processes. Analyses of UVCS observations of CME plasma properties and the evolution of CMEs have provided the following: temperatures, inflow velocities and derived values of resistivity and reconnection rates in CME current sheets, compression ratios and extremely high ion temperatures behind CME shocks, and three dimensional flow velocities and magnetic field chirality in CMEs. Ultraviolet spectroscopy has been used to determine the thermal energy content of CMEs allowing the total energy budget to be known for the first time. Such spectroscopic observations are capable of providing detailed empirical descriptions of solar energetic particle (SEP) source regions that allow theoretical models of SEP acceleration to be tailored to specific events, thereby enabling in situ measurements of freshly emitted SEPs to be used for testing and guiding the evolution of SEP acceleration theory. Here we review the history of ultraviolet coronagraph spectroscopy, summarize the physics of spectral line formation in the extended corona, describe the spectroscopic diagnostic techniques, review the advances in our understanding of solar wind source regions and flare/CME events provided by ultraviolet spectroscopy and discuss the scientific potential of next generation ultraviolet coronagraph spectrometers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkohl@cfa.harvard.edu NR 512 TC 113 Z9 114 U1 2 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 EI 1432-0754 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD APR PY 2006 VL 13 IS 1-2 BP 31 EP 157 DI 10.1007/s00159-005-0026-7 PG 127 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038TG UT WOS:000237251800002 ER PT J AU Elmhamdi, A Danziger, IJ Branch, D Leibundgut, B Baron, E Kirshner, RP AF Elmhamdi, A Danziger, IJ Branch, D Leibundgut, B Baron, E Kirshner, RP TI Hydrogen and helium traces in type Ib-c supernovae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : supernovae : general; line : identification; line : profiles ID IIB SUPERNOVA; IC SUPERNOVAE; OPTICAL-SPECTRA; LIGHT CURVES; TIME SPECTRA; SN 1993J; H-ALPHA; SPECTROSCOPY; EMISSION; PHASE AB Aims. To investigate the spectroscopic properties of a selected optical photospheric spectra of core collapse supernovae (CCSNe). Special attention is devoted to traces of hydrogen at early phases. The impact on the physics and nature of their progenitors is emphasized. Methods. The CCSNe-sample spectra are analyzed with the parameterized supernova synthetic spectrum code "SYNOW" adopting some simplifying approximations. Results. The generated spectra are found to match the observed ones reasonably well, including a list of only 23 candidate ions. Guided by SN Ib 1990I, the observed trough near 6300 angstrom is attributed to Ha in almost all type Ib events, although in some objects it becomes too weak to be discernible, especially at later phases. Alternative line identifications are discussed. Differences in the way hydrogen manifests its presence within CCSNe are highlighted. In type Ib SNe, the H alpha contrast velocity (i.e. line velocity minus the photospheric velocity) seems to increase with time at early epochs, reaching values as high as 8000 km s(-1) around 15-20 days after maximum and then remains almost constant. The derived photospheric velocities, indicate a lower velocity for type II SNe 1987A and 1999em as compared to SN Ic 1994I and SN IIb 1993J, while type Ib events display a somewhat larger variation. The scatter, around day 20, is measured to be similar to 5000 km s-1. Following two simple approaches, rough estimates of ejecta and hydrogen masses are given. A mass of hydrogen of approximately 0.02 M-circle dot is obtained for SN 1990I, while SNe 1983N and 2000H ejected similar to 0.008 M-circle dot and similar to 0.08 M-circle dot of hydrogen, respectively. SN 1993J has a higher hydrogen mass, similar to 0.7 M-circle dot with a large uncertainty. A low mass and thin hydrogen layer with very high ejection velocities above the helium shell, is thus the most likely scenario for type Ib SNe. Some interesting and curious issues relating to oxygen lines suggest future investigations. C1 Abdus Salaam Int Ctr Theoret Phys, I-34014 Trieste, Italy. INAF, Osservatorio Astron Callurania, I-64100 Teramo, Italy. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. European So Observ, D-85478 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Abdus Salaam Int Ctr Theoret Phys, Strada Costiera 11, I-34014 Trieste, Italy. EM elmhamdi@ts.astro.it RI Baron, Edward/A-9041-2009 OI Baron, Edward/0000-0001-5393-1608 NR 58 TC 51 Z9 53 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 APR PY 2006 VL 450 IS 1 BP 305 EP 330 DI 10.1051/0004-6361:20054366 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 029JO UT WOS:000236558700035 ER PT J AU Sozzetti, A Udry, S Zucker, S Torres, G Beuzit, JL Latham, DW Mayor, M Mazeh, T Naef, D Perrier, C Queloz, D Sivan, JP AF Sozzetti, A Udry, S Zucker, S Torres, G Beuzit, JL Latham, DW Mayor, M Mazeh, T Naef, D Perrier, C Queloz, D Sivan, JP TI A massive planet to the young disc star HD 81040 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : planetary systems; stars : individual : HD 81040; stars : activity; stars : abundances; techniques : radial velocities; techniques : spectroscopic ID EXTRA-SOLAR PLANETS; MAIN-SEQUENCE STARS; CA-II H; CORALIE SURVEY; GIANT PLANET; MAGNETIC ACTIVITY; SUBSTELLAR COMPANIONS; DETERMINISTIC MODEL; RADIAL-VELOCITIES; G-DWARF AB We report the discovery of a massive planetary companion orbiting the young disc star HD 81040. Based on five years of precise radial-velocity measurements with the HIRES and ELODIE spectrographs, we derive a spectroscopic orbit with a period P = 1001.0 days and eccentricity e = 0.53. The inferred minimum mass for the companion of m(2) sin i = 6.86 M-Jup places it in the high-mass tail of the extrasolar planet mass distribution. From the ELODIE spectra we derive a Lithium abundance of log epsilon(Li) = 1.90, and from the HIRES spectra of the cores of the Ca II H and K lines we derive an activity index of [log R'(HK)] = - 4.48, suggesting an age of about 0.8 Gyr. The radial-velocity residuals exhibit a scatter significantly larger than the typical internal measurement precision of the instruments. We attribute this excess velocity jitter to activity on the surface of the moderately young host star. However, the amplitude of the jitter is much too small and the expected period of rotation is much too short to explain the observed orbital motion, which we conclude is due to a massive planetary companion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. Observ Geneva, CH-1290 Sauveny, Switzerland. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Dept Geophys & Planetary Sci, IL-69678 Tel Aviv, Israel. Univ Grenoble 1, Lab Astrophys Grenoble, F-38041 Grenoble, France. European So Observ, Santiago 19, Chile. Observ Haute Provence, F-04870 St Michel lObservatoire, France. RP Sozzetti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asozzett@cfa.harvard.edu OI Sozzetti, Alessandro/0000-0002-7504-365X NR 77 TC 18 Z9 18 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 APR PY 2006 VL 449 IS 1 BP 417 EP 424 DI 10.1051/0004-6361:20054303 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 021OD UT WOS:000235991600042 ER PT J AU Jorgensen, JK Johnstone, D van Dishoeck, EF Doty, SD AF Jorgensen, JK Johnstone, D van Dishoeck, EF Doty, SD TI The effect of a strong external radiation field on protostellar envelopes in Orion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; radiative transfer; astrochemistry ID MOLECULAR CLOUD CORES; LOW-MASS PROTOSTARS; PHOTODISSOCIATION REGIONS; LINE EMISSION; PHYSICAL CONDITIONS; INFRARED SOURCES; H2CO ABUNDANCE; NEBULA; ASTROCHEMISTRY; EVOLUTION AB We discuss the effects of an enhanced interstellar radiation field (ISRF) on the observables of protostellar cores in the Orion cloud region. Dust radiative transfer is used to constrain the envelope physical structure by reproducing SCUBA 850 mu m emission. Previously reported (CO)-C-13, (CO)-O-17 and H2CO line observations are reproduced through detailed Monte Carlo line radiative transfer models. It is found that the (CO)-C-13 line emission is marginally optically thick and sensitive to the physical conditions in the outer envelope. An increased temperature in this region is needed in order to reproduce the (CO)-C-13 line strengths and it is suggested to be caused by a strong heating from the exterior, corresponding to an ISRF in Orion 10(3) times stronger than the "standard" ISRF. The typical temperatures in the outer envelope are higher than the desorption temperature for CO. The (CO)-O-17 emission is less sensitive to this increased temperature but rather traces the bulk envelope material. The data are only fit by a model where CO is depleted, except in the inner and outermost regions where the temperature increases above 30 - 40 K. The fact that the temperatures do not drop below approximate to 25 K in any of the envelopes whereas a significant fraction of CO is frozen- out suggest that the interstellar radiation field has changed through the evolution of the cores. The H2CO lines are successfully reproduced in the model of an increased ISRF with constant abundances of 3 - 5 x 10(-10). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. RP Jorgensen, JK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS42, Cambridge, MA 02138 USA. EM jjorgensen@cfa.harvard.edu RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 NR 45 TC 35 Z9 35 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 APR PY 2006 VL 449 IS 2 BP 609 EP 619 DI 10.1051/0004-6361:20053011 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 024MH UT WOS:000236198600025 ER PT J AU Kumar, MSN Keto, E Clerkin, E AF Kumar, MSN Keto, E Clerkin, E TI The youngest stellar clusters - Clusters associated with massive protostellar candidates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; HII regions; open clusters and associations : general ID ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; EMBEDDED STAR-CLUSTERS; HERBIG AE/BE STARS; MOLECULAR OUTFLOWS; ACCRETION; EVOLUTION; OBJECTS; SAMPLE; SEARCH AB We report on the identification of 54 embedded clusters around 217 massive protostellar candidates of which 34 clusters are new detections. The embedded clusters are identified as stellar surface density enhancements in the 2 mu m All Sky Survey (2MASS) data. Because the clusters are all associated with massive stars in their earliest evolutionary stage, the clusters should also be in an early stage of evolution. Thus the properties of these clusters should reflect properties associated with their formation rather than their evolution. For each cluster, we estimate the mass, the morphological type, the photometry and extinction. The clusters in our study, by their association with massive protostars and massive outflows, reinstate the notion that massive stars begin to form after the first generation of low mass stars have completed their accretion phase. Further, the observed high gas densities and accretion rates at the centers of these clusters is consistent with the hypothesis that high mass stars form by continuing accretion onto low mass stars. C1 Univ Porto, Ctr Astrofis, P-7150462 Oporto, Portugal. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kumar, MSN (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-7150462 Oporto, Portugal. EM nanda@astro.up.pt RI Kumar, Nanda/I-4183-2013 NR 64 TC 47 Z9 47 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 APR PY 2006 VL 449 IS 3 BP 1033 EP U138 DI 10.1051/0004-6361:20053104 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 025ET UT WOS:000236248800017 ER PT J AU Wijnands, R in't Zand, JJM Rupen, M Maccarone, T Homan, J Cornelisse, R Fender, R Grindlay, J van der Klis, M Kuulkers, E Markwardt, CB Miller-Jones, JCA Wang, QD AF Wijnands, R in't Zand, JJM Rupen, M Maccarone, T Homan, J Cornelisse, R Fender, R Grindlay, J van der Klis, M Kuulkers, E Markwardt, CB Miller-Jones, JCA Wang, QD TI The XMM-Newton/Chandra monitoring campaign of the Galactic center region - Description of the program and preliminary results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; binaries : close; X-rays : binaries ID X-RAY TRANSIENT; SOURCE 1E 1743.1-2843; NEUTRON-STAR; DISCOVERY; EMISSION; BINARIES; BURSTERS; CATALOG; OSCILLATIONS; BEPPOSAX AB We present the first results of our X-ray monitoring campaign on a 1.7 square degree region centered on Sgr A* using the satellites XMM-Newton and Chandra. The purpose of this campaign is to monitor the behavior (below 10 keV) of X-ray sources (both persistent and transient) which are too faint to be detected by monitoring instruments aboard other satellites currently in orbit (e.g., Rossi X-ray Timing Explorer; INTEGRAL). Our first monitoring observations (using the HRC-I aboard Chandra) were obtained on June 5, 2005. Most of the sources detected could be identified with foreground sources, such as X-ray active stars. In addition we detected two persistent X-ray binaries (1E 1743.1-2843; 1A 1742-294), two faint X-ray transients (GRS 1741.9-2853; XMM J174457-2850.3), as well as a possible new transient source at a luminosity of a few times 10(34) erg s(-1). We report on the X-ray results on these systems and on the non-detection of the transients in follow-up radio data using the Very Large Array. We discuss how our monitoring campaign can help to improve our understanding of the different types of X-ray transients (i.e., the very faint ones). C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Natl Radio Astron Observ, Socorro, NM 87801 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20711 USA. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ESA, ESTEC, ISOC, Madrid 28080, Spain. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM rudy@science.uva.nl; jeanz@sron.nl; mrupen@milkyway.gsfc.nasa.gov; tjm@astro.soton.ac.uk; jeroen@space.mit.edu; cornelis@astro.soton.ac.uk; rpf@phys.soton.ac.uk; josh@cfa.harvard.edu; michiel@science.va.nl; Erik.Kuulkers@esa.int; craigm@milkyway.gsfc.nasa.gov; jmiller@science.uva.nl; wqd@astro.umass.edu RI Miller-Jones, James/B-2411-2013 OI Miller-Jones, James/0000-0003-3124-2814 NR 59 TC 71 Z9 71 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 APR PY 2006 VL 449 IS 3 BP 1117 EP U199 DI 10.1051/0004-6361:20054129 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 025ET UT WOS:000236248800024 ER PT J AU Schwartz, DA Marshall, HL Lovell, JEJ Murphy, DW Bicknell, GV Birkinshaw, M Gelbord, J Georganopoulos, M Godfrey, L Jauncey, DL Perlman, ES Worrall, DM AF Schwartz, DA Marshall, HL Lovell, JEJ Murphy, DW Bicknell, GV Birkinshaw, M Gelbord, J Georganopoulos, M Godfrey, L Jauncey, DL Perlman, ES Worrall, DM TI Chandra observations of magnetic fields and relativistic beaming in four quasar jets SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : general; X-rays : galaxies ID X-RAY JET; ACTIVE GALACTIC NUCLEI; LARGE-SCALE JETS; HUBBLE-SPACE-TELESCOPE; EXTENDED RADIO JETS; SYNCHROTRON RADIATION; 3C-273; CONNECTION; EMISSION; COMPTON AB We discuss the physical properties of four quasar jets imaged with the Chandra X-Ray Observatory in the course of a survey for X-ray emission from radio jets (Marshall et al.). These objects have sufficient counts to study their spatially resolved properties, even in the 5 ks survey observations. We have acquired Australia Telescope Compact Array data with resolution matching Chandra. We have searched for optical emission with Magellan, with sub-arcsecond resolution. The radio to X-ray spectral energy distribution for most of the individual regions indicates against synchrotron radiation from a single-component electron spectrum. We therefore explore the consequences of assuming that the X-ray emission is the result of inverse Compton scattering on the cosmic microwave background. If particles and magnetic fields are near minimum energy density in the jet rest frames, then the emitting regions must be relativistically beamed, even at distances of order 500 kpc from the quasar. We estimate the magnetic field strengths, relativistic Doppler factors, and kinetic energy flux as a function of distance from the quasar core for two or three distinct regions along each jet. We develop, for the first time, estimates in the uncertainties in these parameters, recognizing that they are dominated by our assumptions in applying the standard synchrotron minimum energy conditions. The kinetic power is comparable with, or exceeds, the quasar radiative luminosity, implying that the jets are a significant factor in the energetics of the accretion process powering the central black hole. The measured radiative efficiencies of the jets are of order 10(-4). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 72611, Australia. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head-cfa.harvard.edu RI Godfrey, Leith/B-5283-2013 NR 47 TC 27 Z9 27 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 APR 1 PY 2006 VL 640 IS 2 BP 592 EP 602 DI 10.1086/500102 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300006 ER PT J AU Treu, T Koopmans, LV Bolton, AS Burles, S Moustakas, LA AF Treu, T Koopmans, LV Bolton, AS Burles, S Moustakas, LA TI The sloan lens acs survey. II. Stellar populations and internal structure of early-type lens galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation; galaxies : structure; gravitational lensing ID DIGITAL SKY SURVEY; FIELD ELLIPTIC GALAXIES; SPECTROSCOPIC TARGET SELECTION; DYNAMICALLY HOT GALAXIES; DARK-MATTER HALOS; TO-LIGHT RATIOS; FUNDAMENTAL PLANE; GRAVITATIONAL LENS; INTERMEDIATE-REDSHIFT; RED GALAXIES AB We use HST images to derive effective radii and effective surface brightnesses of 15 early-type (E+S0) lens galaxies identified by the SLACS Survey. Our measurements are combined with stellar velocity dispersions from the SDSS database to investigate for the first time the distribution of lens galaxies in the fundamental plane ( FP) space. Accounting for selection effects ( top priority to the largest Einstein radii and thus approximately to the largest velocity dispersions, sigma greater than or similar to 240 km s(-1)) and for passive evolution, the distribution of the lens galaxies inside the FP is indistinguishable from that of the parent sample of SDSS galaxies. We conclude that SLACS lenses are a fair sample of high velocity dispersion E+S0s. By comparing the central stellar velocity dispersion (sigma) with the velocity dispersion that best fits the lensing models (sigma(SIE)) we find < f(SIE)> equivalent to = 1.01 +/- 0.02 with 0.065 rms scatter. We infer that within the Einstein radii (typically R(e)/2) the SLACS lenses are very well approximated by isothermal ellipsoids, requiring a fine tuning of the stellar and dark matter distribution (the bulge-halo "conspiracy''). Interpreting the offset from the local FP in terms of evolution of the stellar mass-to-light ratio, we find d log (M/L(B))/dz = - 0.69 +/- 0.08 (rms 0.11) consistent with the rate found for field E+S0s and with most of the stars being old (z(f) > 2) and less than similar to 10% of the stellar mass having formed below z = 1. We discuss our results in the context of formation mechanisms such as collisionless ("dry'') mergers. C1 Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Treu, T (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM tt@physics.ucsb.edu; koopmans@astro.rug.nl; bolton@alum.mit.edu; burles@mit.edu; leonidas@jpl.nasa.gov OI Moustakas, Leonidas/0000-0003-3030-2360 NR 92 TC 148 Z9 149 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 APR 1 PY 2006 VL 640 IS 2 BP 662 EP 672 DI 10.1086/500124 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300011 ER PT J AU Vikhlinin, A Kravtsov, A Forman, W Jones, C Markevitch, M Murray, SS Van Speybroeck, L AF Vikhlinin, A Kravtsov, A Forman, W Jones, C Markevitch, M Murray, SS Van Speybroeck, L TI Chandra sample of nearby relaxed galaxy clusters: Mass, gas fraction, and mass-temperature relation SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; dark matter; galaxies : clusters : general; X-rays : galaxies : clusters ID DARK-MATTER HALOS; M-T RELATION; X-RAY-CLUSTERS; COSMOLOGICAL PARAMETERS; INTRACLUSTER MEDIUM; FLUCTUATION SPECTRUM; INFRARED PROPERTIES; SCALING PROPERTIES; PSPC OBSERVATIONS; DENSITY PROFILE AB We present gas and total mass profiles for 13 low-redshift, relaxed clusters spanning a temperature range 0.7 - 9 keV, derived from all available Chandra data of sufficient quality. In all clusters, gas-temperature profiles are measured to large radii (Vikhlinin et al.) so that direct hydrostatic mass estimates are possible to nearly r(500) or beyond. The gas density was accurately traced to larger radii; its profile is not described well by a beta model, showing continuous steepening with radius. The derived rho(tot) profiles and their scaling with mass generally follow the Navarro-Frenk-White model with concentration expected for dark matter halos in Lambda CDM cosmology. However, in three cool clusters, we detect a central mass component in excess of the Navarro-Frenk-White profile, apparently associated with their cD galaxies. In the inner region (r < 0.1r(500)), the gas density and temperature profiles exhibit significant scatter and trends with mass, but they become nearly self-similar at larger radii. Correspondingly, we find that the slope of the mass-temperature relation for these relaxed clusters is in good agreement with the simple self-similar behavior, M-500 proportional to T-alpha, where alpha = (1.5 - 1.6) +/- 0.1, if the gas temperatures are measured excluding the central cool cores. The normalization of this M - T relation is significantly, by approximate to 30%, higher than most previous X-ray determinations. We derive accurate gas mass fraction profiles, which show an increase with both radius and cluster mass. The enclosed f(gas) profiles within r(2500) similar or equal to 0.4r(500) have not yet reached any asymptotic value and are still far (by a factor of 1.5 - 2) from the universal baryon fraction according to the cosmic microwave background (CMB) observations. The f(gas) trends become weaker and its values closer to universal at larger radii, in particular, in spherical shells r(2500) < r < r(500). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow, Russia. Univ Chicago, Enrico Fermi Inst, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avikhlinin@cfa.harvard.edu NR 90 TC 692 Z9 694 U1 0 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 691 EP 709 DI 10.1086/500288 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300013 ER PT J AU Vikhlinin, A AF Vikhlinin, A TI Predicting a single-temperature fit to multicomponent thermal plasma spectra SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : n-body simulations; techniques : spectroscopic; X-rays : galaxies; X-rays : galaxies : clusters ID X-RAY; GALAXY CLUSTERS; EMISSION; CHANDRA; MASS AB Observed X-ray spectra of hot gas in clusters, groups, and individual galaxies are commonly fit with a single-temperature thermal plasma model, although the beam may contain emission from components with different temperatures. Recently, Mazzotta et al. pointed out that thus derived T-spec can be significantly different from commonly used definitions of average temperature, such as emission-weighted or emission measure -weighted T, and found an analytic expression for predicting Tspec for a mixture of plasma spectra with relatively hot temperatures (T greater than or similar to 3 keV). In this paper, we propose an algorithm that can accurately predict T-spec in a much wider range of temperatures (T greater than or similar to 0.5 keV) and for essentially arbitrary abundances of heavy elements. This algorithm can be applied in the deprojection analysis of objects with the temperature and metallicity gradients, for correction of the point-spread function (PSF) effects, for consistent comparison of numerical simulations of galaxy clusters and groups with the X-ray observations, and for estimating how emission from undetected components can bias the global X-ray spectral analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Space Res, Moscow 117997, Russia. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 87 Z9 87 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 710 EP 715 DI 10.1086/500121 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300014 ER PT J AU Kraft, RP Jones, C Nulsen, PEJ Hardcastle, MJ AF Kraft, RP Jones, C Nulsen, PEJ Hardcastle, MJ TI The complex X-ray morphology of NGC 7618: A major group- group merger in the local universe? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 7618); galaxies : ISM; X-rays : galaxies ID EARLY-TYPE GALAXIES; ELLIPTIC GALAXY; CHANDRA OBSERVATION; CLUSTER; CORE; GAS; EINSTEIN; NGC-507; FRONTS AB We present results from a short Chandra ACIS-S observation of NGC 7618, the dominant central galaxy of a nearby (z = 0.017309, d = 74.1 Mpc) group. We detect a sharp surface brightness discontinuity 14.4 kpc north of the nucleus subtending an angle of 130 degrees with an X-ray tail extending similar to 70 kpc in the opposite direction. The temperature of the gas inside and outside the discontinuity is 0.79 +/- 0.03 and 0.81 +/- 0.07 keV, respectively. There is marginal evidence for a discontinuous change in the elemental abundance (Z(inner) = 0.65 +/- 0.25, Z(outer) = 0.17 +/- 0.21 at 90% confidence), suggesting that this may be an "abundance'' front. Fitting a two-temperature model to the ASCA GIS spectrum of the NGC 7618/UGC 12491 pair shows the presence of a second, much hotter (T = similar to 2.3 keV) component. We consider several scenarios for the origin of the edge and the tail, including a radio lobe/IGM interaction, nonhydrostatic "sloshing,'' equal-mass merger and collision, and ram pressure stripping. In the last case, we consider the possibility that NGC 7618 is falling into UGC 12491 or that both groups are falling into a gas-poor cluster potential. There are significant problems with the first two models, however, and we conclude that the discontinuity and tail are most likely the result of ram pressure stripping of the NGC 7618 group, as it falls into a larger dark matter potential. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 28 TC 11 Z9 11 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 762 EP 767 DI 10.1086/500123 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300018 ER PT J AU DeLaney, T Gaensler, BM Arons, J Pivovaroff, MJ AF DeLaney, T Gaensler, BM Arons, J Pivovaroff, MJ TI Time variability in the X-ray nebula powered by pulsar B1509-58 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G320.4-1.2); ISM : jets and outflows; pulsars : individual (B1509-58); stars : neutron; supernova remnants; X-rays : ISM ID CRAB-NEBULA; SUPERNOVA REMNANT; WIND NEBULA; SYNCHROTRON NEBULA; CHANDRA OBSERVATION; SOUTHERN MILKY; PSR B1509-58; VELA PULSAR; MSH 15-52; JET AB We use new and archival Chandra and ROSAT data to study the time variability of the X-ray emission from the pulsar wind nebula (PWN) powered by PSR B1509-58 on timescales of 1 week to 12 yr. There is variability in the size, number, and brightness of compact knots appearing within 2000 of the pulsar, with at least one knot showing a possible outflow velocity of similar to 0.6c (assuming a distance to the source of 5.2 kpc). The transient nature of these knots may indicate that they are produced by turbulence in the flows surrounding the pulsar. A previously identified prominent jet extending 12 pc to the southeast of the pulsar increased in brightness by 30% over 9 yr; apparent outflow of material along this jet is observed with a velocity of similar to 0.5c. However, outflow alone cannot account for the changes in the jet on such short timescales. Magnetohydrodynamic sausage or kink instabilities are feasible explanations for the jet variability, with timescales of similar to 1.3-2 yr. An arc structure located 30"-45" north of the pulsar shows transverse structural variations and appears to have moved inward with a velocity of similar to 0.03c over 3 yr. The overall structure and brightness of the diffuse PWN exterior to this arc and excluding the jet has remained the same over the 12 yr span. The photon indices of the diffuse PWN and possibly the jet steepen with increasing radius, likely indicating synchrotron cooling at X-ray energies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP DeLaney, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tdelaney@cfa.harvard.edu; bgaensler@cfa.harvard.edu; arons@berkeley.edu; pivovaroff1@llnl.gov RI Gaensler, Bryan/F-8655-2010; Pivovaroff, Michael/M-7998-2014; OI Pivovaroff, Michael/0000-0001-6780-6816; Gaensler, Bryan/0000-0002-3382-9558 NR 50 TC 24 Z9 24 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 929 EP 940 DI 10.1086/500189 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300032 ER PT J AU Torres, G Lacy, CH Marschall, LA Sheets, HA Mader, JA AF Torres, G Lacy, CH Marschall, LA Sheets, HA Mader, JA TI The eclipsing binary V1061 Cygni: Confronting stellar evolution models for active and inactive solar-type stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; binaries : spectroscopic; stars : evolution; stars : individual (V1061 Cyg); techniques : spectroscopic ID MAIN-SEQUENCE STARS; INTERMEDIATE ASTROMETRIC DATA; LINED SPECTROSCOPIC BINARIES; LIMB-DARKENING COEFFICIENTS; MIXING-LENGTH PARAMETER; LOW-MASS STARS; ABSOLUTE DIMENSIONS; LATE-F; TEMPERATURE SCALE; MAGNETIC ACTIVITY AB We present spectroscopic and photometric observations of the eclipsing system V1061 Cyg (P = 2.35 days). A third star is visible in the spectrum, and the system is a hierarchical triple. We combine the radial velocities for the three stars, times of eclipse, and intermediate astrometric data from the Hipparcos mission (abscissa residuals) to establish the elements of the outer orbit, which is eccentric and has a period of 15.8 yr. We determine accurate values for the masses, radii, and effective temperatures of the binary components: M-Aa = 1.282 +/- 0.015 M-circle dot, R-Aa = 1.615 +/- 0.017 R-circle dot, and T-eff(Aa) = 6180 +/- 100 K for the primary (star Aa), and M-Ab = 0.9315 +/- 0.0068 M-circle dot, R-Ab = 0.974 +/- 0.020 R-circle dot, and T-eff(Ab) = 5300 +/- 150 K for the secondary (Ab). The mass of the tertiary is determined to be M-B = 0.925 +/- 0.036 M-circle dot and its effective temperature is T-eff(B) = 5670 +/- 150 K. Current stellar evolution models agree well with the properties of the primary but show a very large discrepancy in the radius of the secondary, in the sense that the predicted values are similar to 10% smaller than observed (a similar to 5 sigma effect). In addition, the temperature is cooler than predicted, by some 200 K. These discrepancies are quite remarkable given that the star is only 7% less massive than the Sun, the calibration point of all stellar models. We identify the chromospheric activity as the likely cause of the effect. Inactive stars agree very well with the models, while active ones such as V1061 Cyg Ab appear systematically too large and too cool. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. WM Keck Observ, Kamuela, HI 96743 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; clacy@uark.edu; marschal@gettysburg.edu; holly.a.sheets@dartmouth.edu; jmader@keck.hawaii.edu NR 90 TC 74 Z9 76 U1 1 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 1018 EP 1038 DI 10.1086/500188 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300041 ER PT J AU Lecar, M Podolak, M Sasselov, D Chiang, E AF Lecar, M Podolak, M Sasselov, D Chiang, E TI On the location of the snow line in a protoplanetary disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; planetary systems : protoplanetary disks ID ACCRETION DISKS; GIANT PLANETS; NEBULA; ICE; STARS; EARTH AB In a protoplanetary disk, the inner edge of the region where the temperature falls below the condensation temperature of water is referred to as the snow line. Outside the snow line, water ice increases the surface density of solids by a factor of 4. The mass of the fastest growing planetesimal ( the isolation mass) scales as the surface density to the 3/2 power. It is thought that ice-enhanced surface densities are required to make the cores of the gas giants ( Jupiter and Saturn) before the disk gas dissipates. Observations of our solar system's asteroid belt suggest that the snow line occurred near 2.7 AU. In this paper we revisit the theoretical determination of the snow line. In a minimum-mass disk characterized by conventional opacities and a mass accretion rate of 10(-8) M-circle dot yr(-1), the snow line lies at 1.6 - 1.8 AU, just past the orbit of Mars. The minimum-mass disk, with a mass of 0.02 M-circle dot, has a lifetime of 2 million years with the assumed accretion rate. Moving the snow line past 2.7 AU requires that we increase the disk opacity, accretion rate, and/or disk mass by factors ranging up to an order of magnitude above our assumed baseline values. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Lecar, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Podolak, Morris/0000-0003-4801-8691 NR 23 TC 94 Z9 95 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2006 VL 640 IS 2 BP 1115 EP 1118 DI 10.1086/500287 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RR UT WOS:000236360300049 ER PT J AU Kaplan, DL Gaensler, BM Kulkarni, SR Slane, PO AF Kaplan, DL Gaensler, BM Kulkarni, SR Slane, PO TI An X-ray search for compact central sources in supernova remnants. II. Six large-diameter snrs SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE pulsars : general; stars : neutron; supernova remnants; X rays : stars ID EARLY-TYPE GALAXIES; ALL-SKY SURVEY; BRIGHT SOURCE CATALOG; SIGMA-D RELATION; CYGNUS LOOP; NEUTRON-STARS; CATACLYSMIC VARIABLES; CHANDRA OBSERVATIONS; OPTICAL OBSERVATIONS; RADIO PULSARS AB We present the second in a series of studies in which we have searched for undiscovered neutron stars in supernova remnants ( SNRs). This paper deals with the six largest SNRs in our sample, too large for Chandra or XMM-Newton to cover in a single pointing. These SNRs are nearby, with typical distances of < 1 kpc. We therefore used the ROSAT Bright Source Catalog and past observations in the literature to identify X-ray point sources in and near the SNRs. Out of 54 sources, we were immediately able to identify optical/IR counterparts to 41 from existing data. We obtained Chandra snapshot images of the remaining 13 sources. Of these, 10 were point sources with readily identified counterparts, two were extended, and one was not detected in the Chandra observation but is likely a flare star. One of the extended sources may be a pulsar wind nebula, but if so it is probably not associated with the nearby SNR. We are then left with no identified neutron stars in these six SNRs down to luminosity limits of similar to 10(32) ergs s(-1). These limits are generally less than the luminosities of typical neutron stars of the same ages, but are compatible with some lower luminosity sources such as the neutron stars in the SNRs CTA 1 and IC 443. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Kaplan, DL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave,Room 37-664H, Cambridge, MA 02139 USA. EM dlk@space.mit.edu; bgaensler@cfa.harvard.edu; srk@astro.caltech.edu; slane@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 75 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2006 VL 163 IS 2 BP 344 EP 371 DI 10.1086/501441 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034VG UT WOS:000236958100006 ER PT J AU Jahoda, K Markwardt, CB Radeva, Y Rots, AH Stark, MJ Swank, JH Strohmayer, TE Zhang, W AF Jahoda, K Markwardt, CB Radeva, Y Rots, AH Stark, MJ Swank, JH Strohmayer, TE Zhang, W TI Calibration of the Rossi X-Ray Timing Explorer proportional counter array SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation : detectors; space vehicles : instruments ID FULL-ENERGY ABSORPTION; XENON GAS DETECTORS; GASEOUS XENON; CASSIOPEIA-A; PERFORMANCE; PCA; NONLINEARITY; SIMULATION; SPECTRUM; PULSARS AB We present the calibration and background model for the Proportional Counter Array on board the Rossi X-Ray Timing Explorer. The energy calibration is systematics-limited below 10 keV, with deviations from a power-law fit to the Crab Nebula plus pulsar of less than 1%. Unmodeled variations in the instrumental background amount to less than 2% of the observed background below 10 keV and less than 1% between 10 and 20 keV. Individual photon arrival times are accurate to 4.4 mu s at all times during the mission and to 2.5 mu s after 1997 April 29. The peak pointing direction of the five collimators is known to a precision of a few arcseconds. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Connecticut Coll, Dept Phys & Astron, New London, CT 06320 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lafayette Coll, Dept Phys, Easton, PA 18042 USA. RP Jahoda, K (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. RI Jahoda, Keith/D-5616-2012; Swank, Jean/F-2693-2012; OI Rots, Arnold/0000-0003-2377-2356 NR 38 TC 340 Z9 341 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2006 VL 163 IS 2 BP 401 EP 423 DI 10.1086/500659 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 034VG UT WOS:000236958100009 ER PT J AU James, HF Olson, SL AF James, Helen F. Olson, Storrs L. TI A new species of Hawaiian finch (Drepanidini : Loxioides) from Makauwahi Cave, Kaua'i SO AUK LA English DT Article DE extinction; fossil birds; island biogeography; systematics AB A new species of Hawaiian finch is described from two fossil maxillae recovered from Holocene lacustrine sediments in Makauwahi Cave, island of Kaua'i. The new species is assigned to Loxioides on the basis of characters defined in a previous study of drepanidine phylogeny. The maxilla of the new species resembles that of L. bailleui (the only other member of the genus) in its distinctly foreshortened shape, but differs in size and several qualitative characters. The species was sympatric with Loxioides cf. bailleui during the Holocene on Kaua'i. Like L. bailleuli, it may have been a resource specialist feeding mainly on leguminous pods. The radiocarbon chronology of the Makauwahi site indicates that the species became extinct in the late Holocene and, more tentatively, that it may have survived well beyond the time when humans first discovered and colonized Kaua'i. C1 Museo Nacl Hist Nat, Bird Div, Smithsonian Inst, Washington, DC 20013 USA. RP James, HF (reprint author), Museo Nacl Hist Nat, Bird Div, Smithsonian Inst, Washington, DC 20013 USA. EM jamesh@si.edu NR 23 TC 5 Z9 5 U1 1 U2 2 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 APR PY 2006 VL 123 IS 2 BP 335 EP 344 DI 10.1642/0004-8038(2006)123[335:ANSOHF]2.0.CO;2 PG 10 WC Ornithology SC Zoology GA 041GN UT WOS:000237442500004 ER PT J AU Lampert, KP Bernal, XE Rand, AS Mueller, UG Ryan, MJ AF Lampert, KP Bernal, XE Rand, AS Mueller, UG Ryan, MJ TI No evidence for female mate choice based on genetic similarity in the tungara frog Physalaemus pustulosus SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE animal communication; mate choice; relatedness; microsatellite marker; sexual selection ID MAJOR HISTOCOMPATIBILITY COMPLEX; SEXUAL SELECTION; MATING PREFERENCES; MICROSATELLITE LOCI; MOLECULAR MARKERS; RECEIVER BIASES; EVOLUTION; MHC; RELATEDNESS; HETEROZYGOSITY AB In most sexually reproducing animals, the behavior of one or both sexes during courtship critically influences the success at mating of the opposite sex. This behavior is often interpreted as "mate choice," and there is great interest in why such choices are exercised. The explanation for the evolution of mate choice that has received the most attention and generated the most controversy is based on assumed genetic effects. In this study, we investigated whether female tungara frogs, which choose mates based on acoustic cues, have a preference for genetically less related males. Specifically, we determine if there is disassortive mating based on microsatellite markers, if there is information in the advertisement call that could be used to assess genetic similarity, and if females exhibit acoustic-based mating preferences that would promote choice for genetic diversity. Using seven microsatellite markers, we found no correlation of male call similarity and male genetic relatedness. Female choice experiments showed no female preference for calls of less related males, and there was no evidence for inbreeding avoidance in the field. Our results do not support the hypothesis of mate choice based on information about genetic relatedness conveyed by acoustic signals in tungara frogs. C1 Univ Wurzburg, Dept Physiol Chem 1, D-97074 Wurzburg, Germany. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Lampert, KP (reprint author), Univ Wurzburg, Dept Physiol Chem 1, D-97074 Wurzburg, Germany. EM kathrin.lampert@biozentrum.uni-wuerzburg.de NR 56 TC 14 Z9 14 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD APR PY 2006 VL 59 IS 6 BP 796 EP 804 DI 10.1007/s00265-005-0125-5 PG 9 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 024MR UT WOS:000236199600010 ER PT J AU Paredes, R Jones, IL Boness, DJ AF Paredes, R Jones, IL Boness, DJ TI Parental roles of male and female thick-billed murres and razorbills at the Gannet Islands, Labrador SO BEHAVIOUR LA English DT Article DE parental care; seabird; alcid; chick provisioning; foraging trips; parental roles; sex ID GUILLEMOT URIA-AALGE; ALCA-TORDA; DIVING BEHAVIOR; BRUNNICHS GUILLEMOTS; VOCAL RECOGNITION; METABOLIC-RATES; SEX-DIFFERENCES; FLEDGING MASS; LOMVIA; CARE AB We studied female and male parental roles in two sympatric auks, thick-billed murre (Uric lomvia) and razorbill (Alca torch), with initial biparental care at the breeding site and later exclusively paternal care at sea. Our study addressed the following two questions: Why do males accompany chicks to sea?, and How do the sexes allocate parental effort at the breeding site before parental care at sea begins? We tested the hypothesis that males care for chicks at sea because they are in better condition at the time of chick departure as a result of female-biased parental effort at the breeding site ('nest'). Breeding success and duration of chick-rearing did not differ between the two study years in either species at the Gannet Islands, Labrador. At the breeding colonies, females of both species provided more food (murres: 2.84 +/- 0.18 loads day(-1); razorbills: 2.02 +/- 0.11 loads day(-1)) to their chicks than males (murres: 2.26 +/- 0.12 loads day(-1); razorbills: 1.42 +/- 0.09 loads day(-1)), and males spent more time brooding the chicks. These differences were chick-age dependent in both species, with females providing more meals to chicks older than two weeks. Razorbill males spent more time with chicks greater than two weeks old, while murre male's attentiveness of brooding did not vary with chick age. In both species, males (murres: 3.04 +/- 0.3 h day(-1): razorbill: 3.30 +/- 0.2 h day(-1)) performed longer foraging trips with meal delivery than females (murres: 1.23 +/- 0.4 h/day; razorbill: 2.50 +/- 0.4 h day(-1)). Thick-billed murres showed a consistent diurnal pattern of egg and chick attendance: females were usually found at the breeding site during the day whereas males were found there early in the morning and at night. In contrast, razorbill's timing of attendance was much more variable and did not differ between sexes. Despite these differences in timing of breeding site attendance between species, males of both species spent twice as much time as females engaged in the defence of the egg or chick at the breeding site, which suggest male-biased capability of protecting the chick at departure. Overall our data indicated different female and male parental roles at the breeding site but not a female-biased allocation of time, energy and risk as predicted. In fact, males seem to provide equal if not more parental effort than females prior to the time of colony departure. We propose that the patterns of parental roles found between sexes is the result of a chain of events favouring male involvement in chick brooding and care at sea. C1 Univ Calif Santa Cruz, Inst Marine Sci, Long Marine Lab, Santa Cruz, CA 95060 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Univ Maine, Orono, ME USA. RP Paredes, R (reprint author), Univ Calif Santa Cruz, Inst Marine Sci, Long Marine Lab, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM u92rp@mun.ca NR 72 TC 24 Z9 25 U1 4 U2 14 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PD APR PY 2006 VL 143 BP 451 EP 481 DI 10.1163/156853906776240641 PN 4 PG 31 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 047RF UT WOS:000237895700003 ER PT J AU Medina, E Aguiar, G Gomez, M Aranda, J Medina, JD Winter, K AF Medina, E Aguiar, G Gomez, M Aranda, J Medina, JD Winter, K TI Taxonomic significance of the epicuticular wax composition in species of the genus Clusia from Panama SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE alkanes; Clusia; epicuticular wax; taxonomy; triterpenes; Panama ID ALKANES; BIOSYNTHESIS; EVOLUTION; CAATINGA; GENETICS; CERRADO; PLANTS AB We attempted to separate species of the genus Clusia according to the concentration of linear alkanes (C25 and C35), and the presence and diversity of terpenes in epicuticular wax extracts. We collected leaves of 15 Clusia species growing in mountain forests of Panama (Cerro Jefe 1007 m and Altos de Campana 800 m a.s.l.) and from cultivated plants at two lowland sites. Leaf surfaces were washed gently with hexane to extract epicuticular waxes, which were analyzed using gas chromatography and mass spectrometry. The predominant alkanes were C29, C31, and C33. In the extract the ratio C31/C29 was <= 1 in 6 of the 15 species analyzed: Clusia multiflora, Clusia peninsulae (Hammel ined.), Clusia stenophylla, Clusia liesneri, Clusia coclensis, and Clusia triflora. The concentrations of C29 and C33 were inversely related, the latter being above 10% in Clusia divaricata, Clusia pratensis, Clusia rosea, Clusia uvitana, and Clusia valerioi. Proportion of triterpenes was less than 5% in the species C. minor, C. pratensis, C. uvitana, C. rosea, Clusia cylindrica, C. divaricata, and C. valerioi. The rest contained squalene, and specific triterpenes such as beta-amyrine in C. liesneri, betuline in Clusia osseocarpa, taraxerol in C. stenophylla, and lupeol in C. multiflora. The variety of triterpenes was higher in Clusia liesneri (5) and C. multiflora (3). The results suggest that groups of species can be distinguished within the genus according to the presence of terpenes and ratios of linear alkanes. These groups overlap with those generated by other classifications using morphology and nuclear ribosomal DNA. (C) 2005 Elsevier Ltd. All rights reserved. C1 Inst Venezolano Invest Cient, Ctr Ecol, Caracas 1020A, Venezuela. Inst Venezolano Invest Cient, Ctr Quim, Caracas 1020A, Venezuela. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Medina, E (reprint author), Inst Venezolano Invest Cient, Ctr Ecol, Aptdo 21827, Caracas 1020A, Venezuela. EM cmedina@ivic.ve NR 28 TC 28 Z9 30 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD APR PY 2006 VL 34 IS 4 BP 319 EP 326 DI 10.1016/j.bse.2005.10.009 PG 8 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 029LH UT WOS:000236563400006 ER PT J AU Renner, SC Waltert, M Muhlenberg, M AF Renner, SC Waltert, M Muhlenberg, M TI Comparison of bird communities in primary vs. young secondary tropical montane cloud forest in Guatemala SO BIODIVERSITY AND CONSERVATION LA English DT Article DE avian species richness; conservation; deforestation; diversity; Guatemala; land-use ID ORNITHOLOGISTS UNION CHECKLIST; NORTH-AMERICAN BIRDS; SOUTH-EAST-ASIA; CONSERVATION; DEFORESTATION; BIODIVERSITY; NUMBER; EXTINCTION; SUPPLEMENT; SYSTEMS AB Cloud forests in central Guatemala are fragmented and decreasing in area due to slash-and-burn agricultural activities. We studied bird species composition, abundance, guild composition, and site tenacity of a 102 ha plot located in a cloud forest region of the Sierra Yalijux in Guatemala, half of which was primary forest and half young secondary forest (< 7-years-old). Of the 100 species present 14 were restricted to the Endemic Bird Area 'Northern Central American highlands' (i.e. 66% of a total of 21 endemics). Five of the 100 analysed species, including one of the restricted-range species (Troglodytes rufociliatus), had a significantly different abundance in primary and secondary forests. Theoretical analysis suggests that seven species out of a community comprised of 141 bird species are already extirpated and only three out of the 14 present restricted-range species might survive the current state of deforestation. Insectivores were the dominant guild on the plot in terms of numbers of species, followed by omnivores, frugivores and granivores. However, in terms of individuals, omnivores made up nearly half of the bird individuals in primary forest, but declined by 44% in secondary forest, whereas granivores more than doubled in this habitat type. Numbers of species per guild were not significantly different between habitats, while numbers of individuals per guild were significantly different. In general, individuals per species are significantly different in the two habitats. Results suggest that most of the species that are currently surviving in the remnant forests of the Sierra Yalijux might be fairly well adapted to a range of forest conditions, but that populations of a number of restricted-range species might be small. Even generalists species like the Common Bush Tanager (Chlorospingus ophthalmicus) are less abundant in secondary vegetation than in primary forest of the study plot. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Univ Gottingen, Ctr Nat Conservat, D-37075 Gottingen, Germany. RP Renner, SC (reprint author), Smithsonian Inst, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM renners@crc.si.edu RI Renner, Swen/J-3502-2014; Waltert, Matthias/E-9134-2010 OI Renner, Swen/0000-0002-6893-4219; NR 66 TC 12 Z9 15 U1 4 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2006 VL 15 IS 4 BP 1545 EP 1575 DI 10.1007/s10531-005-2930-6 PG 31 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 055MA UT WOS:000238453600027 ER PT J AU Whigham, DF O'Neill, JP Rasmussen, HN Caldwell, BA McCormick, MK AF Whigham, DF O'Neill, JP Rasmussen, HN Caldwell, BA McCormick, MK TI Seed longevity in terrestrial orchids - Potential for persistent in situ seed banks SO BIOLOGICAL CONSERVATION LA English DT Article DE soil seed bank; terrestrial orchids; Maryland; seed longevity; seed viability ID MYCO-HETEROTROPHIC PLANTS; SYMBIOTIC GERMINATION; MYCORRHIZAL FUNGI; CORALLORHIZA-TRIFIDA; DORMANCY; ECOLOGY AB Terrestrial orchids typically produce numerous small seeds that contain very small nutrient reserves. The seeds are structurally adapted for wind dispersal but little is known about their fate after dispersal. Some studies of seed viability in situ indicate survival for up to two years in temperate orchid species. Seeds stored in the laboratory may last much longer. We investigated seed viability of seven North American orchid species with seed packets buried in a range of soil and wood substrates within their natural habitats. In Goodyera pubescens most seeds germinated within one year. Four other species continued to germinate sparsely during the observation period, but after almost seven years many seeds were still viable. In one species, Liparis liliifolia, seeds that had been in situ for four years had germination rates as high as 68% when sown in vitro with a compatible fungus. The remaining two species did not germinate during the observation period but the seeds were judged to be intact and tested positively for viability after four years in the ground. These observations are interpreted as different species-specific strategies for in situ germination and their seed bank potential is discussed. (c) 2005 Elsevier Ltd. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Danish Forest & Landscape Res Inst, DK-2970 Horsholm, Denmark. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. RP Whigham, DF (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM whighamd@si.edu RI Rasmussen, Hanne/P-5485-2014; OI Rasmussen, Hanne/0000-0002-0181-9304; Whigham, Dennis/0000-0003-1488-820X NR 37 TC 42 Z9 47 U1 4 U2 50 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD APR PY 2006 VL 129 IS 1 BP 24 EP 30 DI 10.1016/j.biocon.2005.10.029 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 025JF UT WOS:000236261000004 ER PT J AU Zotz, G Schmidt, G AF Zotz, G Schmidt, G TI Population decline in the epiphytic orchid Aspasia principissa SO BIOLOGICAL CONSERVATION LA English DT Article DE cost of reproduction; elasticities; growth; Panama; pollinator limitation ID VASCULAR EPIPHYTES; FRUIT PRODUCTION; PHYSIOLOGICAL ECOLOGY; LEPANTHES ORCHIDACEAE; DEMOGRAPHIC APPROACH; PROJECTION MATRIX; TROPICAL FORESTS; LAELIA-RUBESCENS; SLIPPER ORCHID; GENE FLOW AB The population dynamics of the epiphytic orchid Aspasia principissa, growing in the moist tropical forest of Barro Colorado Island, Panama, were studied from 1997 until 2004. Using growth analysis, projection matrix analysis, elasticity analysis, and different types of simulations, we identified the components of the life cycle with the strongest effect on population growth rate (lambda), and related differences in vital rates to environmental variation, mainly in precipitation. Such information, which is almost completely lacking for tropical orchids, is essential for the efficient conservation of these frequently rare and endangered plants. Elasticity analysis indicated that the population growth rate (lambda), which averaged 0.92, was primarily affected by survival, and much less affected by growth or by sexual reproduction. Simulations, which included different levels of pollinator limitation, showed that complete pollination would raise lambda to such an extent as to allow long-term persistence of the population. Pollinator limitation per se, however, is presumably not responsible for the currently observed population decline. Instead, we discuss a possible link between low lambda and (a) a long-term decline in precipitation and (b) recent increases in forest dynamics: variation in annual rainfall significantly affected both recruitment and growth rates of smaller orchid individuals, while the hypothesised increase in the rates of branch and tree falls would increase mortality rates in this epiphyte. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Basel, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. DigiTus iT Serv, D-79576 Weil Am Rhein, Germany. RP Zotz, G (reprint author), Univ Basel, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 65 TC 28 Z9 38 U1 1 U2 13 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD APR PY 2006 VL 129 IS 1 BP 82 EP 90 DI 10.1016/j.biocon.2005.07.022 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 025JF UT WOS:000236261000010 ER PT J AU Carlson, JE Harms, KE AF Carlson, Jane E. Harms, Kyle E. TI The evolution of gender-biased nectar production in hermaphroditic plants SO BOTANICAL REVIEW LA English DT Review ID SENSITIVE FORAGING PREFERENCES; ECHIUM-VULGARE BORAGINACEAE; POLLEN-DONATION HYPOTHESIS; MARGINAL VALUE THEOREM; SEXUAL SELECTION; FLORAL NECTAR; IPOMOPSIS-AGGREGATA; FLOWER COLOR; POLLINATOR VISITATION; ADAPTIVE SIGNIFICANCE AB The evolution of secondary sexual floral traits may be driven by selection through male or female reproductive success. Even so, the gender-biased function of a floral trait is often unapparent because secondary sexual traits and primary sexual organs of both genders co-occur within most bisexual flowers. Within dichogamous plants, however, secondary sexual traits may be unambiguously expressed in association with the primary sexual organs of one gender, making these species uniquely suited to studies of natural and sexual selection on floral traits. The objectives of this article are to summarize patterns of gender-biased nectar production and to critically explore theories relevant to its evolution. We list 41 species with gender-biased nectar production and provide two sets of adaptive hypotheses for the trait: sexual selection hypotheses and inbreeding avoidance hypotheses. We formulate these hypotheses using sexual selection theory in plants and the literature that relates pollinator foraging to plant inbreeding. We also consider explanations based on resource trade-offs, enemies, and genetic correlations. Support for the sexual selection and inbreeding avoidance hypotheses is provided by only a few well-studied species. We outline a series of experiments that should facilitate sorting among hypotheses. Plants with gender-biased nectar production are likely to provide unique insights into the roles of natural and sexual selection in the evolution of floral traits. C1 Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Carlson, JE (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. NR 142 TC 27 Z9 29 U1 2 U2 20 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0006-8101 J9 BOT REV JI Bot. Rev. PD APR-JUN PY 2006 VL 72 IS 2 BP 179 EP 205 DI 10.1663/0006-8101(2006)72[179:TEOGNP]2.0.CO;2 PG 27 WC Plant Sciences SC Plant Sciences GA 062BQ UT WOS:000238919800004 ER PT J AU Sumrall, CD Gahn, FJ AF Sumrall, Colin D. Gahn, Forest J. TI Morphological and systematic reinterpretation of two enigmatic edrioasteroids (Echinodermata) from Canada SO CANADIAN JOURNAL OF EARTH SCIENCES LA English DT Article ID SOUTHERN ONTARIO; MIDDLE ORDOVICIAN; NORTH-AMERICA; NEW-YORK; PALEOECOLOGY; COMMUNITY; LIMESTONES; TAPHONOMY; SHELF AB Reinterpretation of two enigmatic Canadian edrioasteroids, Thresherodiscus ramosus Foerste, 1914 from the Upper Ordovician Verulam Formation of Ontario and Lispidecodus plinthotus Kesling, 1967 from the Lower Mississippian Banff Formation of Alberta, shows that previous accounts of these taxa were largely erroneous. Unlike other isorophid edrioasteroids, Thresherodiscus has branching ambulacra, an unusual hydro-gonopore, differentiated interambulacral plates bearing respiratory structures, and ambulacra that extend onto the peripheral rim. Except for the turreted thecal shape, Lispidecodus is a rather typical discocystinid edrioasteroid. Phylogenetic analysis weakly supports the placement of Thresherodiscus within Agelacrinitidae and strongly places Lispidecodus within Discocystinae. C1 Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Sumrall, CD (reprint author), Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. EM csumrall@utk.edu NR 42 TC 6 Z9 6 U1 0 U2 2 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4077 J9 CAN J EARTH SCI JI Can. J. Earth Sci. PD APR PY 2006 VL 43 IS 4 BP 497 EP 507 DI 10.1139/E05-114 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 060QS UT WOS:000238817300007 ER PT J AU Ross, C Kupper, FC Jacobs, RS AF Ross, C Kupper, FC Jacobs, RS TI Involvement of reactive oxygen species and reactive nitrogen species in the wound response of Dasycladus vermicularis SO CHEMISTRY & BIOLOGY LA English DT Article ID NITRIC-OXIDE SYNTHASE; PLANT-DISEASE RESISTANCE; INDUCED OXIDATIVE BURST; WALL STRUCTURAL PROTEINS; POTATO-TUBER TISSUES; SIGNAL-TRANSDUCTION; ARABIDOPSIS-THALIANA; NITRATE REDUCTASE; HYDROGEN-PEROXIDE; ABSCISIC-ACID AB We investigated the signaling events involved in the wound response of the marine macroalga Dasycladus vermicularis, finding nitric oxide (NO) production in relation to injury. The addition of exogenous H2O2 to aliquots of injured algae accelerated the kinetics of NO production in the wounded region. Similarly, the addition of an NO donor caused an increase in detectable H2O2 around the site of injury. By wounding or incubating uninjured algae with an NO donor, peroxidase activity was enhanced. Based on the use of selected pharmacological probes, our results indicate that H2O2 production involves the upstream activation of signaling events similar to those observed in the physiology of higher plants. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Scottish Assoc Marine Sci, Dunstaffnage Marine Res Lab, Oban PA37 1QA, Argyll, Scotland. Univ Calif Santa Barbara, Interdepartmental Program Marine Sci, Santa Barbara, CA 93106 USA. RP Ross, C (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM ross@sms.si.edu RI Ross, Cliff/B-8291-2011 NR 95 TC 35 Z9 36 U1 0 U2 4 PU CELL PRESS PI CAMBRIDGE PA 1100 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 USA SN 1074-5521 J9 CHEM BIOL JI Chem. Biol. PD APR PY 2006 VL 13 IS 4 BP 353 EP 364 DI 10.1016/j.chembiol.2006.01.009 PG 12 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 040KC UT WOS:000237376400004 PM 16632248 ER PT J AU Beutel, RG Balke, M Steiner, WE AF Beutel, RG Balke, M Steiner, WE TI The systematic position of Meruidae (Coleoptera, Adephaga) and the phylogeny of the smaller aquatic adephagan beetle families SO CLADISTICS LA English DT Review ID LARVAL HEAD STRUCTURES; 18S RIBOSOMAL-RNA; HALIPLIDAE-COLEOPTERA; GYRINIDAE COLEOPTERA; LECONTE COLEOPTERA; MORPHOLOGY; DYTISCIDAE; CHARACTERS; TRACHYPACHIDAE; ASPIDYTIDAE AB A phylogenetic analysis of Adephaga is presented. It is based on 148 morphological characters of adults and larvae and focussed on a placement of the recently described Meruidae, and the genus-level phylogeny of the smaller aquatic families Gyrinidae, Haliplidae and Noteridae. We found a sister group relationship between Gyrinidae and the remaining adephagan families, as was found in previous studies using morphology. Haliplidae are either the sister group of Dytiscoidea or the sister group of a clade comprising Geadephaga and the dytiscoid families. Trachypachidae was placed as the sister group of the rhysodid-carabid clade or of Dytiscoidea. The monophyly of Dytiscoidea including Meru is well supported. Autapomorphies are the extensive metathoracic intercoxal septum, the origin of the metafurca from this structure, the loss of Mm. furcacoxalis anterior and posterior, and possibly the presence of an elongated subcubital setal binding patch. Meruidae was placed as sister group of the Noteridae. Synapomorphies are the absence of the transverse ridge of the metaventrite, the fusion of abdominal segments III and IV, the shape of the strongly asymmetric parameres, and the enlargement of antennomeres 5, 7 and 9. The Meru-noterid clade is the sister group of the remaining Dytiscoidea. The exact position of Aspidytes within this clade remains ambiguous: it is either the sister group of Amphizoidae or the sister group of a clade comprising this family and Hygrobiidae + Dytiscidae. The sister group relationship between Spanglerogyrinae and Gyrininae was strongly supported. The two included genera of Gyrinini form a clade, and Enhydrini are the sister group of a monophylum comprising the remaining Enhydrini and Orectochilini. A branching pattern (Peltodytes + (Brychius + Haliplus)) within Haliplidae was confirmed. Algophilus, Apteraliplus and the Haliplus-subgenus Liaphlus form a clade. The generic status of the two former taxa is unjustified. The Phreatodytinae are the sister group of Noterinae, and Notomicrus (+ Speonoterus), Hydrocoptus, and Pronoterus branch off successively within this subfamily. The search for the larvae of Meru and a combined analysis of morphological and molecular data should have high priority. (c) The Willi Hennig Society 2006. C1 Univ Jena, Inst Spezielle Zool & Evolutionsbiol, D-07743 Jena, Germany. Zool Staatssammlung, D-81247 Munich, Germany. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Smithsonian Inst, Natl Museum Amer Hist, Dept Entomol, Washington, DC 20560 USA. RP Beutel, RG (reprint author), Univ Jena, Inst Spezielle Zool & Evolutionsbiol, D-07743 Jena, Germany. EM b5bero@rz.uni-jena.de OI Beutel, Rolf Georg/0000-0002-0433-7626 NR 109 TC 28 Z9 32 U1 2 U2 4 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0748-3007 J9 CLADISTICS JI Cladistics PD APR PY 2006 VL 22 IS 2 BP 102 EP 131 DI 10.1111/j.1096-0031.2006.00092.x PG 30 WC Evolutionary Biology SC Evolutionary Biology GA 024EA UT WOS:000236176700002 ER PT J AU Crosier, AE Pukazhenthi, BS Henghali, JN Howard, JG Dickman, AJ Marker, L Wildt, DE AF Crosier, AE Pukazhenthi, BS Henghali, JN Howard, JG Dickman, AJ Marker, L Wildt, DE TI Cryopreservation of spermatozoa from wild-born Namibian cheetahs (Acinonyx jubatus) and influence of glycerol on cryosurvival SO CRYOBIOLOGY LA English DT Article DE cheetah; spermatozoa; semen; genome resource banking; cryoprotectant; glycerol ID TERATOSPERMIC DONORS; REPRODUCTIVE STATUS; RESOURCE BANKS; AMERICAN ZOOS; DOMESTIC CAT; SPERM; MORPHOLOGY; EJACULATE; MOTILITY; CONSERVATION AB Sperm cryopreservation is a valuable tool for the genetic management of ex Situ populations. This study was conducted to assess: (1) semen characteristics of wild-born cheetahs; and (2) the impact of three types of glycerol influence (duration of exposure, temperature, and method of addition) on sperm cryosensitivity. To evaluate the impact of duration of glycerol exposure, spermatozoa were incubated in Test Yolk Buffer (TYB) with 4% glycerol at ambient temperature (similar to 22 degrees C) for 15 vs. 60 min before cryopreservation. To evaluate the influence of temperature and method of glycerol addition, spermatozoa were resuspended at ambient temperature either in TYB with 0% glycerol followed by addition of 8% glycerol (1:1 v/v-, at ambient temperature vs. 5 degrees C) or directly in TYB with 4% glycerol. Ail samples were cryopreserved in straws over liquid nitrogen vapor and evaluated for sperm motility and acrosomal integrity after thawing. Semen, samples (n = 23, 17 = 13 mates) contained a high proportion (78%) of pleiomorphic spermatozoa. Ejaculates also contained a high proportion of acrosome-intact (86%) and motile spermatozoa (78%). Immediately after thawing, a significant proportion of spermatozoa retained intact acrosomes (range.. 48-67%) and motility (range, 40-49%). After thawing, incubation in glycerol for 60 min at ambient temperature before freezing decreased (p < 0.05) sperm motility and acrosomal integrity at one time-point each (pre-centrifugation and post-centrifugation, respectively). However, method or temperature of glycerol addition had no (p > 0.05) impact on sperm cryosurvival. In summary, (1) wild-born cheetahs produce high proportions of piciomorphic spermatozoa but with a high proportion of intact acrosomes; and (2) resuspension in 4% glycerol, followed by exposure for up to 60 min at ambient temperature, had minimal effect on sperm motility and acrosomal integrity after cryopreservation. Results indicate the feasibility of cryopreserving cheetah spermatozoa under field conditions, providing a user-friendly method to capture and store gametes to enhance genetic management. Published by Elsevier Inc. C1 Smithsonians Natl Zool Pk & Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. Cheetah Conservat Fund, Otjiwarongo, Namibia. RP Crosier, AE (reprint author), Smithsonians Natl Zool Pk & Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. EM crosiera@si.edu FU NCRR NIH HHS [K01 RR00135] NR 41 TC 40 Z9 42 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 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD APR PY 2006 VL 52 IS 2 BP 169 EP 181 DI 10.1016/j.cryobiol.2005.10.011 PG 13 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 030AK UT WOS:000236605300001 PM 16412415 ER PT J AU McCormick, MK Whigham, DF Sloan, D O'Malley, K Hodkinson, B AF McCormick, MK Whigham, DF Sloan, D O'Malley, K Hodkinson, B TI Orchid-fungus fidelity: a marriage meant to last? SO ECOLOGY LA English DT Article DE environmental change; Goodyera; mycorrhiza; orchid; Orchidaceae; Tulasnella ID ARBUSCULAR MYCORRHIZAL FUNGI; MYCO-HETEROTROPHIC PLANTS; TERRESTRIAL ORCHIDS; SPECIFICITY; INDIVIDUALS; CHRONOSEQUENCE; ASSOCIATION; COMMUNITIES; NITROGEN; ECOLOGY AB The characteristics of plant-rnycorrhizae associations are known to vary in both time and space, but the ecological consequences of variation in the dynamics of plant-fungus interactions are poorly understood. For example, do plants associate with single fungi or multiple fungi simultaneously, and do the associations persist through a plant's lifetime or do plants support a succession of different fungi? We investigated these and other questions related to plant-fungus interactions in Goodyera pubescens, an evergreen terrestrial orchid of the eastern United States, that interdicts with closely related fungi in the genus Tulasnella. Unlike the mycorrhizal associations of other plants, orchid-mycorrhizal associations only benefit the orchid, based on current evidence. Many terrestrial orchids have been found to associate with specific groups of fungi. This characteristic could potentially limit orchids to relatively narrow ranges of environmental conditions and may be a contributing factor in the decline of many orchids in the face of changing environmental conditions. We found that G. pubescens protocorms (developing embryos prior to leaf production) and adults associated with only one fungal individual at a time. The orchid-fungus association persists for years, but during I drought period that was associated with the death of many plants, surviving plants were able to switch to new fungal individuals. These results. suggest that G. pubescens interacts with the same fungal partner during periods of modest environmental variation but is able to switch to a different fungal partner. We hypothesize that the ability to switch fungi allows G. pubescens to survive more extreme environmental perturbations. However, laboratory experiments suggest that switching fungi has potential costs, as it increases the risk of mortality, especially for smaller individuals. Our findings indicate that it is unlikely that switching fungi is a common way to improve tolerance of less severe environmental fluctuations and disturbances. These findings may have important implications for plant responses to severe climatic events or to more gradual environmental changes such its global warming. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Sloan, Daniel/D-4152-2011; OI Whigham, Dennis/0000-0003-1488-820X NR 37 TC 69 Z9 75 U1 2 U2 34 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD APR PY 2006 VL 87 IS 4 BP 903 EP 911 DI 10.1890/0012-9658(2006)87[903:OFAMMT]2.0.CO;2 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 033QF UT WOS:000236863200013 PM 16676534 ER PT J AU Murphy, KR Ruiz, GM Dunsmuir, WTM Waite, TD AF Murphy, KR Ruiz, GM Dunsmuir, WTM Waite, TD TI Optimized parameters for fluorescence-based verification of ballast water exchange by ships SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID DISSOLVED ORGANIC-MATTER; EXCITATION; PARAFAC; SPECTROSCOPY; SEAWATER; SPECTRA; CDOM; DOC AB Mid-ocean ballast water exchange is mandatory for ships discharging foreign ballast in US territorial waters in order to reduce the risk of biological invasions. However, a reliable tool for determining whether the procedure took place is lacking. We investigated chromophoric dissolved organic matter (CDOM) fluorescence as a tracer of mid-ocean exchange on nine research cruises out of Asia, Europe, and the USA, focusing on challenging source conditions (high salinity, low CDOM). Using parallel factor analysis, we identified nine independent fluorescent components present in varying concentrations in the ocean and in ballast water. One component was sufficient for predicting the coastal vs oceanic source of most ballast water samples. Across nine cruises, thresholds (1.7 and 0.7 ppb quinine sulfate equivalent units) at two fixed wavelength pairs (lambda(ex)/lambda(em) = 320/414 and 370/496 nm, respectively) discriminated coastal from oceanic ballast water in >95% of samples (N = 514). Our results suggest that single- and dual-channel fluorometers could be optimized for verifying ballast water exchange. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ New S Wales, Sch Math, Sydney, NSW 2052, Australia. Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia. RP Murphy, KR (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM murphyka@si.edu RI Murphy, Kathleen/B-8217-2009; Waite, T. David/A-1400-2008; OI Murphy, Kathleen/0000-0001-5715-3604; Waite, T. David/0000-0002-5411-3233; Ruiz, Gregory/0000-0003-2499-441X NR 24 TC 75 Z9 83 U1 3 U2 38 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 1 PY 2006 VL 40 IS 7 BP 2357 EP 2362 DI 10.1021/es0519381 PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 031GC UT WOS:000236691600054 PM 16646474 ER PT J AU Collin, R AF Collin, R TI Sex ratio, life-history invariants, and patterns of sex change in a family of protandrous gastropods SO EVOLUTION LA English DT Article DE Bostrycapulus; calyptraeidae; Crepidula; protandry ID THALASSOMA-BIFASCIATUM PISCES; LYSMATA-WURDEMANNI DECAPODA; CORAL-REEF FISH; SIMULTANEOUS HERMAPHRODITE; CALYPTRAEID GASTROPODS; BLUEHEAD WRASSE; PHENOTYPIC PLASTICITY; SIZE ADVANTAGE; SOCIAL-CONTROL; FEMALE CHOICE AB Application of optimality theory to the evolution of life histories has been broadly successful in predicting the conditions favoring sex change, the type of change, and the timing of such changes. The size advantage hypothesis predicts that the optimal size at which an individual should change sex is a function of its size and the size and sex of its potential mates. I collected data on the size, sex, and grouping of individuals of 27 populations of 19 species of the calyptraeids, a family of protandrous marine gastropods that includes Crepidula. These data are used to test the following predictions about variation in size at sex change: (1) sex ratio is biased toward the first sex; (2) the ratio of the size at sex change to the maximum size is a life-history invariant; and (3) species that form variable-sized groups or stacks have more variation in size at sex change than species that show less variation in stack formation. Across all 19 species, sex ratio was not significantly more often biased toward the first sex than it was toward the second sex, although sex ratios were significantly male biased more often than they were significantly female biased. Sex ratios ranged from 0.05 to 0.91, and this variation was related to mode of development, skew in size distribution, and frequency of stacking, but not with maximum body size. There was little evidence that the ratio of size at sex change and maximum size is invariant. There is evidence that one of the main underlying assumptions of this life-history invariant, that male fertility increases with the same function of size in all species, is invalid for calyptraeids and probably for other animals. Finally, species that form larger stacks or mating groups had more variation in size at sex change within a population than species that were generally solitary. These results suggest that information about individual groupings should be included in predictions of life-history theory and that more information about the relationship between male fitness and size is also needed. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Aprtado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 NR 56 TC 34 Z9 35 U1 3 U2 17 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD APR PY 2006 VL 60 IS 4 BP 735 EP 745 DI 10.1111/j.0014-3820.2006.tb01152.x PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 041GC UT WOS:000237441300009 PM 16739455 ER PT J AU Guinotte, JM Orr, J Cairns, S Freiwald, A Morgan, L George, R AF Guinotte, JM Orr, J Cairns, S Freiwald, A Morgan, L George, R TI Will human-induced changes in seawater chemistry alter the distribution of deep-sea scleractinian corals? SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID ANTHROPOGENIC CO2; LOPHELIA-PERTUSA; CARBON; OCEAN; CALCIFICATION; REEF; IMPACTS AB The answer to the title question is uncertain, as very few manipulative experiments have been conducted to test how deep-sea scleractinians (stony corals) react to changes in seawater chemistry. Ocean pH and calcium carbonate saturation are decreasing due to an influx of anthropogenic CO2 to the atmosphere. Experimental evidence has shown that declining carbonate saturation inhibits the ability of marine organisms to build calcium carbonate skeletons, shells, and tests. Here we put forward a hypothesis suggesting that the global distribution of deep-sea scleractinian corals could be limited in part by the depth of the aragonite saturation horizon (ASH) in the world's oceans. Aragonite is the metastable form of calcium carbonate used by scleractinian corals to build their skeletons and the ASH is the limit between saturated and undersaturated water. The hypothesis is tested by reviewing the distribution of deep-sea, bioherm-forming scleractinian corals with respect to the depth of the ASH. Results indicate that > 95% of 410 coral locations occurred in saturated waters during pre-industrial times. Projections indicate that about 70% of these locations will be in undersaturated waters by 2099. Lab experimentation, in situ experimentation, and monitoring efforts are needed to quantify the effects of changing seawater chemistry on deep-sea coral ecosystems. C1 Marine Conservat Biol Inst, Bellevue, WA USA. James Cook Univ N Queensland, Sch Trop Environm Studies & Geog, Townsville, Qld 4811, Australia. Lab Sci Climat & Environm, Paris, France. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Erlangen Nurnberg, Inst Paleontol, D-8520 Erlangen, Germany. George Inst Biodivers & Sustainabil, Wilmington, NC USA. RP Guinotte, JM (reprint author), Marine Conservat Biol Inst, 2122 112th Ave NE, Bellevue, WA USA. EM john@mcbi.org OI Orr, James/0000-0002-8707-7080; Freiwald, Andre/0000-0002-2335-4042 NR 29 TC 184 Z9 189 U1 5 U2 73 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD APR PY 2006 VL 4 IS 3 BP 141 EP 146 DI 10.1890/1540-9295(2006)004[0141:WHCISC]2.0.CO;2 PG 6 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 031BK UT WOS:000236678900018 ER PT J AU Hawley, DM Lindstrom, K Wikelski, M AF Hawley, DM Lindstrom, K Wikelski, M TI Experimentally increased social competition compromises humoral immune responses in house finches SO HORMONES AND BEHAVIOR LA English DT Article DE social competition; dominance status; immunocompetence; corticosterone; sheep red blood cells; house finches ID MYCOPLASMA-GALLISEPTICUM INFECTION; CARPODACUS-MEXICANUS; HEMATOLOGICAL PARAMETERS; PARASITIC INFECTION; STRESS RESPONSES; SEASONAL-CHANGES; LIZARD MORPHS; TRADE-OFFS; HOST; POPULATION AB Although social behavior can substantially influence an individual's physiology, few studies have examined whether intraspecific competition compromises individual immunocompetence. We experimentally manipulated the intensity of social competition in captive non-breeding house finches (Carpodacus mexicanus) by supplying few (high competition) or many (low competition) feeding sites. We tested whether elevated levels of social competition caused individual changes in aggression rates, humoral immunity, body mass, and baseline and stress-induced corticosterone concentrations. We also examined whether physiological responses to social competition were related to an individual's social status. We found that house finches under high social competition had significantly higher aggression rates, lower antibody responses, and lost more body mass. Within flocks, dominant individuals mounted stronger immune responses in both competition treatments. Our statistical power to detect differences in circulating corticosterone concentrations was low, but we did not find any support for the hypothesis that corticosterone concentrations mediate immunosuppression among or within flocks: baseline and stress-induced corticosterone concentrations did not differ under high and low social competition, were unrelated to individual social status, and did not predict the extent of immunosuppression among individuals. Overall, we documented that two universal components of social behavior, intraspecific competition and social status, modulated the strength of a humoral immune response in house finches. (C) 2005 Elsevier Inc. All rights reserved. C1 Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Hawley, DM (reprint author), Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, Washington, DC 20008 USA. EM dmh35@cornell.edu OI Hawley, Dana/0000-0001-9573-2914 NR 65 TC 25 Z9 26 U1 1 U2 26 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0018-506X J9 HORM BEHAV JI Horm. Behav. PD APR PY 2006 VL 49 IS 4 BP 417 EP 424 DI 10.1016/j.yhbeh.2005.09.003 PG 8 WC Behavioral Sciences; Endocrinology & Metabolism SC Behavioral Sciences; Endocrinology & Metabolism GA 028IO UT WOS:000236480700001 PM 16256991 ER PT J AU Durrant, KL Hughes, JM AF Durrant, KL Hughes, JM TI Are there correlates of male Australian Magpie Gymnorhina tibicen reproductive success in a population with high rates of extra-group paternity? SO IBIS LA English DT Article ID RED-WINGED BLACKBIRDS; PAIR PATERNITY; TERRITORY QUALITY; PLUMAGE COLORATION; BLOOD PARASITES; PARENTAL EFFORT; PARUS-MAJOR; MATE CHOICE; GREAT TITS; GOOD-GENES AB The reproductive success of a male bird is often correlated with measurable traits that predict his intrinsic quality. Females are thought to base their selection of mates on the latter's 'quality' in order to gain their 'good genes'. Male Australian Magpies Gymnorhina tibicen of the white-backed race tyrannica were trapped in two breeding seasons. Measurements were taken of morphometric and other characteristics in order to discover whether particular traits of males were associated with: (1) percentage of offspring sired in the territory, (2) number of fledglings produced in the territory per season and (3) whether females select males for their 'good genes'. There were no consistently significant correlations between any of the measured variables and male Magpie reproductive success within territories. In particular, none of the traits measured had any consistent correlation with the percentage of offspring sired in a territorial group. This was an unexpected result given that the species is strongly territorial but also engages regularly in extra-group copulations. These findings appear contrary to the predictions of the 'good genes' hypothesis. The general lack of correlation between the variables and level of genetic paternity may in fact be due to females engaging in extra-group mating primarily to avoid breeding with a close relative rather than to choose a high-quality male. In this case, males would not have to be 'high quality', but merely genetically different from the female's social mate. C1 Griffith Univ, Australian Sch Environm Studies, Nathan, Qld 4111, Australia. RP Durrant, KL (reprint author), Smithsonian Inst, Natl Zool Pk, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM durrantk@si.edu NR 43 TC 4 Z9 4 U1 3 U2 15 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0019-1019 J9 IBIS JI Ibis PD APR PY 2006 VL 148 IS 2 BP 313 EP 320 PG 8 WC Ornithology SC Zoology GA 032TV UT WOS:000236798700013 ER PT J AU Valencia, D O'Connell, RJ Sasselov, D AF Valencia, D O'Connell, RJ Sasselov, D TI Internal structure of massive terrestrial planets SO ICARUS LA English DT Article DE extrasolar planets; interiors; terrestrial planets ID GIANT PLANETS; EARTH; CORE; CONSTRAINTS; ACCRETION; MODEL AB Planetary formation models predict the existence of massive terrestrial planets and experiments are now being designed that should succeed in discovering them and measuring their masses and radii. We calculate internal structures of planets with one to ten times the mass of the Earth (Super-Earths) to obtain scaling laws for total radius, mantle thickness, core size and average density as a function of mass. We explore different compositions and obtain a scaling law of R proportional to M0.267-0-272 for super-Earths. We also study a second family of planets, Super-Mercuries with masses ranging from one mercury-mass to ten mercury-masses with similar composition to the Earth's but with a larger core mass fraction. We explore the effect of surface temperature and core mass fraction on the scaling laws for these planets. The scaling law obtained for the Super-Mercuries is R proportional to (similar to 0.3). (c) 2005 Elsevier Inc. All rights reserved. C1 Harvard Univ, Dept Astron, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Valencia, D (reprint author), Harvard Univ, Dept Astron, Harvard Smithsonian Ctr Astrophys, 20 Oxford St, Cambridge, MA 02138 USA. EM valencia@mail.geophysics.harvard.edu NR 34 TC 215 Z9 216 U1 5 U2 28 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2006 VL 181 IS 2 BP 545 EP 554 DI 10.1016/j.icarus.2005.11.021 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032AF UT WOS:000236745600017 ER PT J AU Rinkevich, FD Zhang, L Hamm, RL Brady, SG Lazzaro, BP Scott, JG AF Rinkevich, FD Zhang, L Hamm, RL Brady, SG Lazzaro, BP Scott, JG TI Frequencies of the pyrethroid resistance alleles of Vssc1 and CYP6D1 in house flies from the eastern United States SO INSECT MOLECULAR BIOLOGY LA English DT Article DE insecticide resistance; population genetics; Musca domestica; Vssc1; CYP6D1; kdr ID SODIUM-CHANNEL GENE; INSECTICIDE RESISTANCE; KNOCKDOWN-RESISTANCE; MUSCA-DOMESTICA; FLY DIPTERA; PERMETHRIN RESISTANCE; BLATTELLA-GERMANICA; SUSCEPTIBLE STRAINS; MOLECULAR ANALYSIS; CROSS-RESISTANCE AB House flies were collected from four dairies in Maine, New York, North Carolina, and Florida, where high levels of resistance to permethrin have been documented. Regions of two genes, CYP6D1 and Vssc1, having alleles that confer resistance to permethrin (and other pyrethroids) were analysed from individuals at each collection site. The combinations of resistance alleles for Vssc1 and CYP6D1 were highly variable between each state. The resistance allele CYP6D1v1 was found at a high frequency (0.63-0.91) at all sites. Individuals homozygous susceptible for CYP6D1 were very rare and detected only at the dairy in Maine. In addition to the typical Vssc1 mutation responsible for resistance, kdr (L1014F), we also identified individuals with a L1014H mutation. Although house flies homozygous for the L1014H mutation had a lower level of resistance to permethrin, compared to L1014F, the H1014 resistance allele was frequently detected. No individuals with the super-kdr allele (M918T + L1014F) were detected from the field collections. The intron 3 bp downstream of the kdr mutation was found to be extremely variable, providing an opportunity to reconstruct a phylogeny of Vssc1 alleles. Based on this analysis it appears the kdr-his mutation had multiple evolutionary origins, but that the kdr mutation may have had a single origin. The impacts of these findings on resistance management are discussed. C1 Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. Smithsonian Inst, Dept Entomol, Suitland, MD 20746 USA. Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Scott, JG (reprint author), Cornell Univ, Dept Entomol, Comstock Hall, Ithaca, NY 14853 USA. EM JGS5@cornell.edu RI Rinkevich, Frank/H-4919-2011 FU NIGMS NIH HHS [GM47835] NR 45 TC 32 Z9 42 U1 1 U2 11 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1075 J9 INSECT MOL BIOL JI Insect Mol. Biol. PD APR PY 2006 VL 15 IS 2 BP 157 EP 167 DI 10.1111/j.1365-2583.2006.00620.x PG 11 WC Biochemistry & Molecular Biology; Entomology SC Biochemistry & Molecular Biology; Entomology GA 028BK UT WOS:000236460300006 PM 16640726 ER PT J AU Reuther, JD Lowenstein, JM Gerlach, SC Hood, D Scheuenstuhl, G Ubelaker, DH AF Reuther, JD Lowenstein, JM Gerlach, SC Hood, D Scheuenstuhl, G Ubelaker, DH TI The use of an improved pRIA technique in the identification of protein residues SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE protein radioimmunoassay; protein residue; experimental archaeology; archaeological applications ID EXPERIMENTAL STONE TOOLS; BLOOD RESIDUES; ARCHAEOLOGICAL MATERIALS; CAUTIONARY NOTE; ROCK-ART; DNA; AUSTRALIA; RECOVERY; SURFACES; ORIGIN AB Blood and protein residue identification in archaeological research has been a controversial subject for the last 20 years. This paper reports oil the use of in improved protein radioimmunoassay (pRIA) technique in identifying protein residues. Results from the blind testing of the original and improved pRIA techniques in identifying bloodstains oil experimental lithic artifacts are described and compared. We argue that the improved pRIA technique is highly sensitive and accurate for identifying protein residues to genus. and thus has excellent applications for archaeological research. (c) 2005 Elsevier Ltd. All rights reserved. C1 No Land Use Res Inc, Fairbanks, AK 99709 USA. Calif Pacific Med Ctr, Dept Nucl Med, San Francisco, CA 94115 USA. Univ Alaska Fairbanks, Dept Chem & Biochem, Dept Anthropol, Fairbanks, AK 99705 USA. MicroAnalyt LLC, Miami, FL 33155 USA. NMNH, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Reuther, JD (reprint author), No Land Use Res Inc, 600 Univ Ave,Suite 6, Fairbanks, AK 99709 USA. EM josh_reuther@yahoo.com; jlowen@itsa.ucsf.edu NR 35 TC 13 Z9 13 U1 2 U2 11 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD APR PY 2006 VL 33 IS 4 BP 531 EP 537 DI 10.1016/j.jas.2005.09.008 PG 7 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 025IB UT WOS:000236257700009 ER PT J AU Klose, SM Smith, CL Denzel, AJ Kalko, EKV AF Klose, Stefan M. Smith, Carolynn L. Denzel, Andrea J. Kalko, Elisabeth K. V. TI Reproduction elevates the corticosterone stress response in common fruit bats SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE glucocorticoids; reproduction; behaviour; phyllostomidae; Chiroptera ID LIFE-HISTORY EVOLUTION; SEASONAL-CHANGES; ARTIBEUS-JAMAICENSIS; TRADE-OFFS; ADRENOCORTICAL RESPONSES; NEOTROPICAL BAT; PASSERINE BIRDS; BASE-LINE; GLUCOCORTICOIDS; CHIROPTERA AB Changes in reproductive state or the environment may affect the sensitivity of the hypothalamic-pituitary-andrenal (HPA) axis. However, little is known about the dynamics of the resulting corticosteroid stress response, in particular in tropical mammals. In this study, we address the modulation of corticosterone release in response to different reproductive conditions and seasonality in 326 free-living common fruit-eating bats (Artibeus jamaicensis) on Barro Colorado Island in Panama during dry and wet seasons. We present strong evidence that stress sensitivity is primarily modulated by reproductive condition. In reproductively active females, corticosterone increases were more rapid and reached higher levels, but also decreased significantly faster than in inactive females. The corticosterone response was weaker in reproducing males than in females and delayed compared to non-reproductive males. Testes volume in reproductively active males was negatively correlated with corticosterone concentrations. Our findings suggest differentiated dynamics in the corticosterone stress response between sexes, potentially reflecting conflicting ecological demands. In females, a strong acute corticosterone response may represent high stress- and risk-sensitivity that facilitates escape and thus helps to protect reproduction. In males, suppression during reproductive activity could reflect lowered stress sensitivity to avoid chronically elevated corticosterone levels in times of frequent aggressive and therefore costly inter-male encounters. C1 Univ Ulm, Dept Expt Ecol, Ecol Endocrinol Lab, D-89069 Ulm, Germany. Univ Queensland, Sch Integrat Biol, Brisbane, Qld 4072, Australia. Macquarie Univ, Dept Biol, Sydney, NSW 2109, Australia. Natl Sci Fdn, Biol Sci Directorate, Arlington, VA 22230 USA. Univ Ulm, Dept Gen Zool & Endorcrinol, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Klose, SM (reprint author), Univ Ulm, Dept Expt Ecol, Ecol Endocrinol Lab, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM stefan.klose@uni-ulm.de OI Smith, Carolynn/0000-0003-4377-5490 NR 69 TC 10 Z9 10 U1 0 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD APR PY 2006 VL 192 IS 4 BP 341 EP 350 DI 10.1007/s00359-005-0067-4 PG 10 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 045GE UT WOS:000237729800001 PM 16273409 ER PT J AU Powell, DM Danze, DE Gwinn, MA AF Powell, DM Danze, DE Gwinn, MA TI Predictors of biting fly harassment and its impact on habitat use by feral horses (Equus caballus) on a barrier island SO JOURNAL OF ETHOLOGY LA English DT Article DE horses; fly; Barrier Island; habitat use; harassment ID CAMARGUE HORSES; SOCIAL-BEHAVIOR; SELFISH HERD; SALT-MARSH; DEER FLIES; PARASITES; DIPTERA; TABANIDAE; DESERT AB Feral horses on Assateague Island, Maryland, were observed in June and August 2000 to determine what behavioral and ecological factors affect the intensity of biting fly harassment and whether habitat use by horses was influenced by biting flies. Fly counts and frequencies of comfort movements (i.e., movements designed to dislodge insects) were recorded during focal animal samples, as well as data on sex, group size, habitat type, temperature, humidity, wind speed, and behavior. Seasonal habitat use patterns were assessed using 7 years of monthly census data on the horses. The number of biting flies on the horse was affected by horse sex, habitat, temperature, and group size. The number of comfort movements a horse showed was affected by habitat, temperature, wind speed, group size, and number of horses within one body length of the focal. The number of comfort movements made by a horse was found to be highly correlated with fly numbers. Though marshes were used most throughout the year, the pattern of use of dune, scrub, and human-altered habitats reflects a pattern of biting fly avoidance and refuge-seeking by the horses. C1 Bronx Zoo, Wildlife Conservat Soc, Dept Mammal, Bronx, NY 10460 USA. Smithsonian Inst, Off Chief Technol Officer, Adm Management Syst Support Branch, Washington, DC 20013 USA. Georgetown Univ, Dept Biol, Washington, DC 20057 USA. RP Powell, DM (reprint author), Bronx Zoo, Wildlife Conservat Soc, Dept Mammal, 2300 Southern Blvd, Bronx, NY 10460 USA. EM dpowell@wcs.org NR 22 TC 3 Z9 3 U1 2 U2 11 PU SPRINGER TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0771 J9 J ETHOL JI J. Ethol. PD APR PY 2006 VL 24 IS 2 BP 147 EP 153 DI 10.1007/s10164-005-0174-2 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 034UG UT WOS:000236955500007 ER PT J AU Abbene, IJ Culver, SJ Corbett, DR Buzas, MA Tully, LS AF Abbene, Irene J. Culver, Stephen J. Corbett, D. Reide Buzas, Martin A. Tully, Lance S. TI Distribution of foraminifera in Pamlico Sound, North Carolina, over the past century SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID CONTINENTAL-SHELF; MARSH FORAMINIFERA; AMAZON SHELF; USA; DYNAMICS; TRACERS; ESTUARY; PB-210; SYSTEM; RIVER AB Foraminiferal and radionuclide data have been used to investigate environmental change that has occurred within Pamlico Sound, North Carolina, over the last century. Environmental conditions were evaluated for three time slices; (1) the modern environment as determined by surficial (0-1 cm) sediments, (2) short-core intervals representing approximately 40 years BP, as determined by Cs-137 activity, and (3) short-core intervals representing approximately 120 years BP, as determined by Pb-210 activity. Cluster analysis distinguished four foraminiferal assemblages at the surface (0-1 cm): (1) Marsh Biofacies, (2) Estuarine Biofacies A, (3) Estuarine Biofacies B, and (4) Marine Biofacies. The Marsh Biofacies is characterized by typical marsh foraminifera such as Tiphotrocha comprimata, Trochammina inflata, Miliammina fusea and Haplophragmoides wilberti. Estuarine Biofacies A is distinguished from Estuarine Biofacies B by the greater relative abundance of the agglutinated species Ammotium salsum and Ammobaculites crassus in the former and the greater relative abundance of Elphidium excavatum in the latter. The Marine Biofacies is comprised completely of calcareous foraminifera (e.g., Elphidium excavatum, Hanzawaia strattoni, Cibicides lobatulus, Elphidium subareticum, Quinqueloculina seminula and Elphidium galvestonense) and is restricted to tidal inlets. Down-core foraminiferal data indicate that approximately 120 years BP, Pamlico Sound was dominated by Estuarine Biofacies A, which is indicative of brackish conditions. Upcore in the 40 years BP and modern time slices, Estuarine Biofacies B is the more prominent assemblage within Pamlico Sound; this is indicative of increased salinity over time. Lowered salinity conditions 120 years BP may be the result of high hurricane activity over a several year period. C1 E Carolina Univ, Dept Geol, Greenville, NC 27858 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Abbene, IJ (reprint author), US Geol Survey, WRD, 2045 Route 112,Bldg 4, Coram, NY 11727 USA. EM culvers@ecu.edu NR 48 TC 26 Z9 27 U1 4 U2 14 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 APR PY 2006 VL 36 IS 2 BP 135 EP 151 DI 10.2113/36.2.135 PG 17 WC Paleontology SC Paleontology GA 046SF UT WOS:000237830600004 ER PT J AU Petrizzo, MR Huber, BT AF Petrizzo, Maria Rose Huber, Brian T. TI Biostratigraphy and taxonomy of late Albian planktonic foraminifera from ODP Leg 171B (western North Atlantic Ocean) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID ANOXIC EVENTS; ENVIRONMENTS; EVOLUTION; SECTION AB A detailed taxonomic and biostratigraphic analysis of upper Albian planktonic foraminifera is presented for Ocean Drilling Program sites 1050 and 1052, which were deposited at similar to 23 degrees N paleolatitude and similar to 1300 m and 300 m paleodepths, respectively, on the Blake Nose escarpment (subtropical western North Atlantic Ocean). The generally excellent preservation of the material, especially in the clay-rich layers, permits recognition of new bioevents within the uppermost Albian, in addition to most of the standard bioevents that have been previously defined in the Tethyan Realm. The taxonomic assignments and the stratigraphic range of some species that are often overlooked or misidentified in the stratigraphic record have also been clarified, and three species are formally described as new (Hedbergella astrepta, H. praelibyca and H. blakensis). Graphic correlation and age-depth curves constructed from integrated planktonic foraminifera and calcareous nannofossils datum events enable reliable estimation of the relative timing of species first and last occurrences and relative abundance variations, as well as determination of the timing and extent of an unconformity at Site 1050. While most of the species datum events are well correlated, several are found to be diachronous and/or unreliable probably as a result of different surface water conditions along the depth transect. C1 Univ Milan, Dipartimento Sci Terra, I-20133 Milan, Italy. Smithsonian Museum Nat Hist, Dept Paleobiol, MRC NHB 121, Washington, DC 20013 USA. RP Petrizzo, MR (reprint author), Univ Milan, Dipartimento Sci Terra, Via Mangiagalli 34, I-20133 Milan, Italy. EM mrose.petrizzo@unimi.it RI Petrizzo, Maria Rose/M-8672-2013 OI Petrizzo, Maria Rose/0000-0002-9584-8471 NR 50 TC 21 Z9 22 U1 0 U2 3 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 APR PY 2006 VL 36 IS 2 BP 166 EP 190 DI 10.2113/36.2.166 PG 25 WC Paleontology SC Paleontology GA 046SF UT WOS:000237830600006 ER PT J AU Cardini, A Thorington, RW AF Cardini, A Thorington, RW TI Postnatal ontogeny of marmot (Rodentia, Sciuridae) crania: Allometric trajectories and species divergence SO JOURNAL OF MAMMALOGY LA English DT Article DE allometry; 2-dimensional and 3 dimensional geometric morphometrics; Marmota; ontogeny; Petromarmota; species divergence ID YELLOW-BELLIED MARMOTS; MORPHOLOGICAL EVOLUTION; GEOMETRIC MORPHOMETRICS; SEXUAL-DIMORPHISM; PHYLOGENY; SHAPE; SOCIALITY; PATTERNS; FLAVIVENTRIS; SQUIRRELS AB Marmots are the largest extant representatives of the squirrel family (Sciuridae). Members of this clade are believed to have conservative skeletal characters and are inclined to convergence in species with similar size and ecology. However, this does not seem to hold for the mandible and cranium of marmots; instead, similarities reflect subgeneric classification or geographic distribution. To understand the pattern of morphological evolution in the genus Marmota, the ontogeny of the cranium is investigated in 7 of the 14 living marmot species. In particular, the role of allometry in producing intra- and interspecific differences is analyzed. Sexual dimorphism in allometric trajectories is found to be negligible, whereas shape traits that characterize a specific age are mostly allometric. Allometry accounts for an important proportion, although not for the majority, of shape variation during postnatal ontogeny of the cranium. Interspecific differences in allometric trajectories are generally small and the majority of shape differences in relation to phylogeny appear early in ontogeny. Thus, allometry might have had a limited role in producing the morphological variation of living marmot species or it might even have constrained the range of evolutionary changes in this clade. A very different role of allometry as a source of morphological novelties can be speculated to exist in earlier stages of man-not evolutionary history, when a highly distinctive cranial shape evolved concomitant with a 2-fold increase in size. Three sets of analyses are performed to investigate the ontogeny of cranial form in Marmota. Three-dimensional (3D) coordinates of anatomical landmarks are used to describe the whole man-not cranium in the first 3D geometric morphometric analysis of a sciurid taxon. Also, anatomical landmarks that describe the dorsal and lateral sides of the cranium are used for 2-dimensional (2D) analyses complementary to previous studies on the ventral cranium. Despite the complexity of the cranium, which makes it a poor candidate for 2D studies, results of 2D and 3D analyses are generally in good agreement. C1 Univ York, Hull York Med Sch, York YO10 5DD, N Yorkshire, England. Univ Hull, Kingston Upon Hull HU6 7RX, N Humberside, England. Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Cardini, A (reprint author), Univ York, Hull York Med Sch, York YO10 5DD, N Yorkshire, England. EM alcardini@interfree.it RI Rohlf, F/A-8710-2008; cardini, andrea/G-9951-2011 OI cardini, andrea/0000-0003-2910-632X NR 54 TC 31 Z9 32 U1 0 U2 4 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD APR PY 2006 VL 87 IS 2 BP 201 EP 215 DI 10.1644/05-MAMM-A-242R1.1 PG 15 WC Zoology SC Zoology GA 037DB UT WOS:000237125800002 ER PT J AU Thies, W Kalko, EKV Schnitzler, HU AF Thies, W Kalko, EKV Schnitzler, HU TI Influence of environment and resource availability on activity patterns of Carollia castanea (Phyllostomidae) in Panama SO JOURNAL OF MAMMALOGY LA English DT Article DE activity patterns; bat; lunar phobia; moonlight; Phyllostomidae ID BAT EPTESICUS-SEROTINUS; COMMON VAMPIRE BAT; FORAGING BEHAVIOR; FRUGIVOROUS BAT; HABITAT USE; ARTIBEUS-JAMAICENSIS; HAREM MAINTENANCE; MYOTIS-LUCIFUGUS; SOUTHERN ENGLAND; MICROHABITAT USE AB Behavioral patterns of animals correlate with biotic (i.e., resources and conspecifics) and abiotic (i.e., weather and lunar cycle) factors. We studied the influence of ambient light, rain, sex, and resource availability on the activity pattern of the neotropical chestnut short-tailed bat (Carollia castanea; Phyllostomidae) in a tropical lowland forest in Panama. Time of emergence was tightly correlated with local sunset, in contrast to the time of return, which occurred sporadically over a span of hours. Activity by individuals peaked at the beginning of the night, coinciding with maximum availability of ripe fruits from understory pepper plants (Piperaceae), their main food source. Bats continued to forage during light and moderate rain and only stopped at heavy rain. Nightly activity level was similar in nonreproductive female and male C. castanea but the temporal distribution of activity differed. Females were more active in the 1st half of night, whereas activity of males was more evenly distributed throughout the night. In contrast to fruit-eating bats in the canopy, C. castanea did not exhibit a significant reduction in flight activity (lunar phobia) during bright nights around the full moon. We conclude that ecological conditions (availability of food and predation risk) and physiological constraints (small body size associated with high metabolic rate) are the most important factors that account for the observed activity patterns. C1 Univ Ulm, D-89069 Ulm, Germany. Univ Tubingen, D-72076 Tubingen, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Kalko, EKV (reprint author), Univ Ulm, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM elisabeth.kalko@uni-ulm.de NR 68 TC 30 Z9 32 U1 0 U2 22 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD APR PY 2006 VL 87 IS 2 BP 331 EP 338 DI 10.1644/05-MAMM-A-161R1.1 PG 8 WC Zoology SC Zoology GA 037DB UT WOS:000237125800018 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI V-2: A combat ifistory of the first ballistic missile. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, 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 APR PY 2006 VL 70 IS 2 BP 548 EP 549 DI 10.1353/jmh.2006.0115 PG 2 WC History SC History GA 028HX UT WOS:000236478900054 ER PT J AU Launius, RD AF Launius, RD TI Into the unknown together: The DOD, NASA, and early spaceflight. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 APR PY 2006 VL 70 IS 2 BP 558 EP 559 DI 10.1353/jmh.2006.0105 PG 2 WC History SC History GA 028HX UT WOS:000236478900062 ER PT J AU Langley, HD AF Langley, HD TI Letters to the Editor SO JOURNAL OF MILITARY HISTORY LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 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 APR PY 2006 VL 70 IS 2 BP 583 EP 583 PG 1 WC History SC History GA 028HX UT WOS:000236478900072 ER PT J AU Gurgel, CF Terada, R Abbott, IA Fredericq, S Norris, JN AF Gurgel, C. F. Terada, R. Abbott, I. A. Fredericq, S. Norris, J. N. TI Towards a global phylogeography of Gracilaria salicornia (gracilariaceae, rhodophyta), an invasive species in Hawaii, based on chloroplast and mitochondrial markers SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL USA. Kagoshima Univ, Fac Fisheries, Shimoarata, Japan. Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. Univ Louisiana, Dept Biol, Lafayette, LA USA. Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RI Gurgel, Carlos/E-6897-2014; Terada, Ryuta/O-2813-2013 OI Gurgel, Carlos/0000-0003-3989-1704; Terada, Ryuta/0000-0003-3193-6592 NR 0 TC 0 Z9 0 U1 0 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2006 VL 42 SU 1 MA 38 BP 13 EP 13 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 161HH UT WOS:000246004900039 ER PT J AU Littler, MM Littler, DS AF Littler, M. M. Littler, D. S. TI Assessment of coral reefs using herbivory/nutrient assays and indicator groups of benthic primary producers: A critical synthesis, proposed protocols, and critique of management strategies SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. Harbor Branch Oceanog Inst Inc, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2006 VL 42 SU 1 MA 40 BP 13 EP 14 PG 2 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 161HH UT WOS:000246004900041 ER PT J AU Cooney, S Stoecker, DK Coats, D AF Cooney, S. Stoecker, D. K. Coats, D. TI Effects of host size and sex on the dinoflagellate gill parasite Crepidoodinium cyprinodontum SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 Univ Maryland, Ctr Environm Sci, Marine Estuarine Environm Sci Program, Cambridge, MD USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2006 VL 42 SU 1 MA 93 BP 29 EP 29 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 161HH UT WOS:000246004900094 ER PT J AU Wysoczanski, RJ Wright, IC Gamble, JA Hauri, EH Luhr, JF Eggins, SM Handler, MR AF Wysoczanski, RJ Wright, IC Gamble, JA Hauri, EH Luhr, JF Eggins, SM Handler, MR TI Volatile contents of Kermadec Arc-Havre Trough pillow glasses: Fingerprinting slab-derived aqueous fluids in the mantle sources of arc and back-arc lavas SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Kermadec Arc-Havre Trough; pillow basalt glass; volatile elements; aqueous slab fluids; subduction zone ID TAUPO VOLCANIC ZONE; CARBON-DIOXIDE SOLUBILITIES; TRACE-ELEMENT TRANSPORT; SUBDUCTED OCEANIC-CRUST; RIDGE BASALTIC LIQUIDS; NEW-ZEALAND; SW PACIFIC; ISLAND-ARC; DEHYDRATION PROCESSES; MAGMA PETROGENESIS AB Aqueous fluids and sediment melts from subducting oceanic lithosphere are the driving force for the refertilisation of the mantle overlying subduction zones. Volatile elements in particular play an important role in the generation of aqueous fluids and the transport of fluid mobile elements. Here we report volatile contents of quenched glasses from pillow-lava rims in the Kermadec Arc-Havre Trough subduction system to provide constraints on the source, generation, and composition of slab-derived aqueous fluids. Water (similar to 1.5 wt.% in glasses, 2.5 wt.% in two melt inclusions), carbon (up to 16 ppm in glasses, 180 ppm in one inclusion) and sulphur (< 700 ppm) contents of all glasses are consistent with degassing of volatiles, which migrated from the melt, through growing vesicles, and into the water column, even in samples collected at depths of up to 3000 m. By contrast, halogen contents have not been affected by degassing or any other secondary processes such as assimilation of seawater. Fluorine contents (250-520 ppm) can be obtained almost entirely from melting of depleted mantle similar to that which generates mid-ocean ridge basalt. However, C1 (650-3000 ppm) is enriched tenfold compared to depleted mantle-derived lavas. A minimum of 70% H2O, > 80% Ba and Pb, and > 98% of C1 is required to be derived from aqueous slab-derived fluids. We propose a single homogenous reservoir for the aqueous fluid source. This reservoir is most likely to be hydrated serpentinite formed above the subducting slab by fluids derived from altered oceanic crust and subducting sediment. Dehydration of the serpentinite occurs as it descends into the mantle, transporting fluid mobile elements into the overlying mantle and triggering partial melting. The similarity of aqueous fluid compositions derived for other oceanic arcs suggests that this process may occur in arc systems worldwide. (c) 2005 Elsevier B.V. All rights reserved. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. Natl Inst Water & Atmosphere Res, Wellington, New Zealand. Natl Univ Ireland Univ Coll Cork, Dept Geol, Cork, Ireland. Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 2601, Australia. Japan Agcy Marine Earth Sci & Technol Ctr, Inst Res Earth Evolut, Yokosuka, Kanagawa 2370061, Japan. RP Wysoczanski, RJ (reprint author), Smithsonian Inst, Dept Mineral Sci, NHB-119, Washington, DC 20560 USA. EM richardw@jamstec.go.jp RI Wright, Ian/B-9643-2008; Wysoczanski, Richard/C-2930-2009; Handler`, Monica/E-9460-2011; Wysoczanski, Richard/I-7730-2012; Eggins, Stephen/H-6943-2016 OI Wright, Ian/0000-0002-6660-0493; Handler`, Monica/0000-0001-7095-0835; Eggins, Stephen/0000-0002-0007-5753 NR 76 TC 34 Z9 35 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 EI 1872-6097 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD APR 1 PY 2006 VL 152 IS 1-2 BP 51 EP 73 DI 10.1016/j.jvolgeores.2005.04.021 PG 23 WC Geosciences, Multidisciplinary SC Geology GA 027XG UT WOS:000236448800003 ER PT J AU Rosenshein, EB Ivanova, MA Dickinson, TL McCoy, TJ Lauretta, DS Guan, Y Leshin, LA Benedix, GK AF Rosenshein, EB Ivanova, MA Dickinson, TL McCoy, TJ Lauretta, DS Guan, Y Leshin, LA Benedix, GK TI Oxide-bearing and FeO-rich clasts in aubrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ENSTATITE CHONDRITES; IGNEOUS ORIGIN; INCLUSIONS; CLASSIFICATION; ACHONDRITES; METEORITES; OLDHAMITE; METAL; CAS AB We report the occurrence of an oxide-bearing clast and an FeO-rich clast from aubrites. The FeO-rich clast in Pesyanoe is dominated by olivine and pyroxene phenocrysts with mineral compositions slightly less FeO-rich than is typical for H chondrites. In Allan Hills (ALH),84008, the oxide-bearing clast consists of a single forsterite grain rimmed by an array of sulfides, oxides, and phosphides. We consider a number of possible origins. We call exclude formation by melting of oxide-bearing chondrules and CAIs formed in enstatite chondrites. The Pesyanoe clast may have formed in a more oxidized region of the aubrite parent body or, more likely, is a foreign clast from a more oxidized parent body. The ALH 84008 clast likely formed by reaction between sulfides and silicates as a result of cooling, oxidation, or de-sulfidization. This clast appears to be the first oxide-bearing clast from an aubritic breccia that formed oil the aubrite parent body. Identification of additional oxide-bearing clasts in aubrites could shed light oil whether this was a widespread phenomenon and the origin of these enigmatic objects. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. SUNY Binghamton, Dept Geol & Environm Sci, Binghamton, NY 13902 USA. Vernadsky Inst Geochem, Lab Meteorit, Moscow 119991, Russia. Natl Acad, Washington, DC 20001 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM mccoyt@si.edu OI Benedix, Gretchen/0000-0003-0990-8878 NR 30 TC 4 Z9 4 U1 0 U2 2 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 APR PY 2006 VL 41 IS 4 BP 495 EP 503 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 038IF UT WOS:000237212300001 ER PT J AU Zhou, SL Renner, SS Wen, J AF Zhou, SL Renner, SS Wen, J TI Molecular phylogeny and intra- and intercontinental biogeography of Calycanthaceae SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Review DE Bayesian divergence time estimation; biogeography; Calycanthaceae; internal transcribed spacer; penalized likelihood; trnC-trnD intergenic spacer; trnL intron; trnL-trnF intergenic spacer ID IDIOSPERMUM-AUSTRALIENSE IDIOSPERMACEAE; LENGTH DIFFERENCE TEST; NUCLEAR RIBOSOMAL DNA; PLASTID GENE RBCL; ANGIOSPERM PHYLOGENY; NUCLEOTIDE-SEQUENCES; NORTHERN-HEMISPHERE; NONCODING REGIONS; UNIVERSAL PRIMERS; CHLOROPLAST DNA AB Based on nuclear and chloroplast sequences we resolve species relationships in Calycanthaceae and develop a biogeographic hypothesis that explains their intercontinental disjunctions and intra-continental diversification in eastern Asia. Fossil-calibrated penalized likelihood and Bayesian divergence time estimates indicate that the Northern Hemisphere Calycanthus and Chimonanthus diverged from each other in the mid-Miocene, while the Australian Idiospermum had already diverged by the Upper Cretaceous and likely represents a remnant of a former Gondwanan distribution of Calycanthaceae that included South America, as indicated by the occurrence of Cretaceous Calycanthaceae fossils in Brazil. Relationships within Calycanthus were difficult to resolve, but a shared 155-bp deletion in the trnL-F intergenic spacer unites the two North American species, which were also sisters in a cpPNA restriction site study. Their ancestor apparently crossed the Bering land bridge in the Miocene. The six species of Chimonanthus, by contrast, diverged from each other as recently as 1-2 my ago, and a DIVA analysis with four areas of endemism recognized within China suggests three vicariance and two dispersal events within Chimonanthus, with initial vicariance having Occurred between eastern and southwestern or central China. Further divergence then appears to have involved eastern and southcentral China, and southwestern and central China. (c) 2006 Elsevier Inc. All rights reserved. C1 Chinese Acad Sci, Inst Bot, Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. Univ Munich, Dept Biol, D-80638 Munich, Germany. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC166, Washington, DC 20013 USA. EM wenj@si.edu NR 107 TC 40 Z9 42 U1 1 U2 12 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 APR PY 2006 VL 39 IS 1 BP 1 EP 15 DI 10.1016/j.ympev.2006.01.015 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 029AU UT WOS:000236531000001 PM 16495090 ER PT J AU Whittall, JB Medina-Marino, A Zimmer, EA Hodges, SA AF Whittall, JB Medina-Marino, A Zimmer, EA Hodges, SA TI Generating single-copy nuclear gene data for a recent adaptive radiation SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE nuclear intron; 3 '-UTR; Aquilegia; orthology; gene genealogy ID REPRODUCTIVE ISOLATION; EVOLUTIONARY BIOLOGY; INTRON SEQUENCES; SPECIES FLOCK; PHYLOGENY; DIVERSIFICATION; SPECIATION; MARKERS; UTILITY; ORIGIN AB Recent adaptive radiations provide an exceptional opportunity to understand the processes of speciation and adaptation. However, reconstructing the phylogenetic history of recent and rapidly evolving clades often requires the use of multiple, independent gene genealogies. Nuclear introns are an obvious source of the necessary data but their use is often limited because degenerate primers can amplify paralogous loci. To identify PCR primers for a large number of loci in an especially rapid adaptive radiation, that of the flowering plant genus Aquilegia (Ranunculaceae), we developed an efficient method for amplifying multiple single-copy nuclear loci by sequencing a modest number of clones from a cDNA library and designing PCR primers; with one primer anchored in the 3' untranslated region (3'-UTR) and one primer in the coding region of each gene. Variation between paralogous loci evolves more quickly in 3'-UTR regions compared to adjacent exons, and therefore we achieved high specificity for isolating orthologous loci. Furthermore, we were able to identify genes containing large introns by amplifying genes from genomic DNA and comparing the PCR product size to that predicted from their cDNA sequence. In Aquilegia eight out of eleven loci were isolated with this method and six of these loci had introns. Among four genes sequenced for samples spanning the phylogenetic breadth of the genus, we found sequence variation at levels similar to that observed in ITS, further supporting the recent and rapid radiation in Aquilegia. We assessed the orthology of amplification products by phylogenetic congruence among loci, the presence of two well established phylogenetic relationships, and similarity among loci for levels of sequence variation. Higher levels of variation among samples for one locus suggest possible paralogy. Overall, this method provides an efficient means of isolating predominantly single-copy loci from both low and high-copy gene families, providing ample nuclear variation for reconstructing species-level phylogenies in non-model taxa. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Smithsonian Inst, Support Ctr, Natl Museum Nat Hist, Dept Bot, Suitland, MD USA. Smithsonian Inst, Support Ctr, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD USA. RP Hodges, SA (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM hodges@lifesci.ucsb.edu RI Zimmer, Elizabeth/G-3890-2011 NR 53 TC 49 Z9 51 U1 2 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD APR PY 2006 VL 39 IS 1 BP 124 EP 134 DI 10.1016/j.ympev.2005.10.010 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 029AU UT WOS:000236531000009 PM 16314114 ER PT J AU Ellis, SC O'Sullivan, E AF Ellis, SC O'Sullivan, E TI Correlations of near-infrared, optical and X-ray luminosity for early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : fundamental parameters; galaxies : general ID COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT CLUSTERS; ELLIPTIC GALAXIES; MULTIPARAMETRIC ANALYSIS; EINSTEIN SAMPLE; STELLAR POPULATIONS; FUNDAMENTAL PLANE; DISTANT CLUSTERS; FIELD GALAXIES; COOLING FLOWS AB The relation between X-ray luminosity and near-infrared (NIR) luminosity for early-type galaxies has been examined. NIR luminosities should provide a superior measure of stellar mass compared to optical luminosities used in previous studies, especially if there is significant star formation or dust present in the galaxies. However, we show that the X-ray-NIR relations are remarkably consistent with the X-ray-optical relations. This indicates that the large scatter of the relations is dominated by scatter in the X-ray properties of early-type galaxies, and is consistent with early-types consisting of old, quiescent stellar populations. We have investigated scatter in terms of environment, surface brightness profile, Mg-2, H beta, H gamma line strength indices, spectroscopic age and nuclear H alpha emission. We found that galaxies with high Mg-2 index, low H beta and H gamma indices or a ` core' profile have a large scatter in LX, whereas galaxies with low Mg-2, high H beta and H gamma indices or ` power-law' profiles generally have L-X < 10(41) erg s(-1). There is no clear trend in the scatter with environment or nuclear Ha emission. C1 Anglo Australian Observ, Epping, NSW 2121, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ellis, SC (reprint author), Anglo Australian Observ, POB 296, Epping, NSW 2121, Australia. EM sce@aao.gov.au OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 84 TC 48 Z9 48 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 1 PY 2006 VL 367 IS 2 BP 627 EP 645 DI 10.1111/j.1365-2966.2005.09982.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 022OG UT WOS:000236064800013 ER PT J AU Kornicker, LS Harrison-Nelson, E AF Kornicker, LS Harrison-Nelson, E TI Ostracoda (Myodocopina) of Tutuila, American Samoa SO PACIFIC SCIENCE LA English DT Article AB Three species (two new) of myodocopid Ostracoda are reported from Tutuila, American Samoa: Paravargula trifax Kornicker, 1991; Cypridina mellentini Kornicker & Harrison-Nelson, n. sp.; and Asteropterygion samoa Kornicker & Harrison-Nelson, n. sp. Only C. mellentini was abundant. The genus Asteropterygion is reported for the first time from a southwestern central Pacific island. Paravargula trifax had been reported previously from Enewetak. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM kornickl@si.edu; nelsone@si.edu NR 19 TC 2 Z9 2 U1 0 U2 1 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD APR PY 2006 VL 60 IS 2 BP 243 EP 259 DI 10.1353/psc.2006.0008 PG 17 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 025VX UT WOS:000236296200007 ER PT J AU Trapani, J Sanders, WJ Mitani, JC Heard, A AF Trapani, J Sanders, WJ Mitani, JC Heard, A TI Precision and consistency of the taphonomic signature of predation by crowned hawk-eagles (Stephanoaetus coronatus) in Kibale National Park, Uganda SO PALAIOS LA English DT Article ID GYRFALCON FALCO-RUSTICOLUS; MULTIPLE CARNIVORE TAXA; BONE ASSEMBLAGES; SOUTH-AFRICA; BIRD BONES; CAPE PROVINCE; TOOTH MARKS; FOREST; INVOLVEMENT; MONKEYS AB Prey material, which was collected from beneath the nests of two pairs of crowned hawk-eagles (Stephanoaetus coronatus) in the Ngogo study area, Kibale National Park, Uganda, was analyzed to identify the taphonomic features diagnostic of eagle predation. Material from a recent three-year collection interval was compared to an earlier three-year collection subsample to determine signal consistency over time. The bulk of the assemblage is comprised of cercopithecoid monkey remains, reflecting the taxonomic composition of the Agogo area. Taxonomic composition of the assemblage remains highly consistent over the collection period. Bone survivability and fragmentation profiles, as well as damage patterns, also were investigated. Crowned hawk-eagles inflict much less damage to prey skeletons than do mammalian carnivores. Crania, scapulae, and hindlimb elements are most likely to survive predation by crowned hawk-eagles and to be concentrated at nest sites, but these elements (especially crania) show age-specific patterns of fragmentation and damage. Bone survivability profiles remain highly consistent throughout the duration of the collection period. Fragmentation and damage patterns-when tallied quantitatively-are more variable, but do not resemble those expected under predation by mammalian carnivores. Regurgitated elements in hair boluses also were examined, when compared with the rest of the assemblage, they show very different patterns. In summary, crowned hawk-eagle predation provides a taphonomic signature distinguishable from those of other predatory accumulating agents (e.g., non-human mammalian carnivores, owls, and humans), and this signal remains consistent over time, leading to the expectation that it may remain intact in fossil assemblages. C1 Smithsonian Inst, Dept Paleobiol, Museum Natl Hist Nat, Washington, DC 20013 USA. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. RP Trapani, J (reprint author), Smithsonian Inst, Dept Paleobiol, Museum Natl Hist Nat, POB 37012, Washington, DC 20013 USA. EM jtrapani@umich.edu NR 73 TC 13 Z9 13 U1 2 U2 7 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD APR PY 2006 VL 21 IS 2 BP 114 EP 131 DI 10.2110/palo.2005.p05-46 PG 18 WC Geology; Paleontology SC Geology; Paleontology GA 037SU UT WOS:000237168100002 ER PT J AU Juarros, E Pellegrini, P Kirby, K Cote, R AF Juarros, E Pellegrini, P Kirby, K Cote, R TI One-photon-assisted formation of ultracold polar molecules SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; HYDROGEN-ATOMS; LITHIUM; LIH AB Alkali-metal hydride molecules have large dipole moments in their ground electronic states. We explore the possibility of forming such molecules from a mixture of the ultracold atomic gases, employing a one-photon stimulated radiative association process. Using accurate molecular potential-energy curves and dipole moments, we have calculated the rate coefficients for populating each of the vibrational levels of the X (1)Sigma(+) states of LiH and NaH. We have found that significant molecule formation rates into the upper vibrational levels can be realized with laser intensities and atomic densities that are easily attainable experimentally. We examine the spontaneous emission cascade which takes place from these upper vibrational levels on a time scale of milliseconds, and calculate the resulting rotational populations in v=0. We show that photon emission in the cascade process does not contribute to trap loss and that a large population of molecules in v=0 can be achieved. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Juarros, E (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. NR 17 TC 20 Z9 20 U1 0 U2 3 PU AMERICAN 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 APR PY 2006 VL 73 IS 4 AR 041403 DI 10.1103/PhysRevA.73.041403 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 037LG UT WOS:000237147700013 ER PT J AU Cernusak, LA Hutley, LB Beringer, J Tapper, NJ AF Cernusak, LA Hutley, LB Beringer, J Tapper, NJ TI Stem and leaf gas exchange and their responses to fire in a north Australian tropical savanna SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Eucalyptus; re-fixation; stem respiration ID CARBON-ISOTOPE DISCRIMINATION; WOODY-TISSUE RESPIRATION; KAKADU NATIONAL-PARK; BRANCH MAINTENANCE RESPIRATION; SEASONAL-CHANGES; CONTRASTING CLIMATES; PLANT RESPIRATION; RAINFALL GRADIENT; PINE FOREST; XYLEM SAP AB We measured stem CO2 efflux and leaf gas exchange in a tropical savanna ecosystem in northern Australia, and assessed the impact of fire on these processes. Gas exchange of mature leaves that flushed after a fire showed only slight differences from that of mature leaves on unburned trees. Expanding leaves typically showed net losses of CO2 to the atmosphere in both burned and unburned trees, even under saturating irradiance. Fire caused stem CO2 efflux to decline in overstory trees, when measured 8 weeks post-fire. This decline was thought to have resulted from reduced availability of C substrate for respiration, due to reduced canopy photosynthesis caused by leaf scorching, and to priority allocation of fixed C towards reconstruction of a new canopy. At the ecosystem scale, we estimated the annual above-ground woody-tissue CO2 efflux to be 275 g C m(-2) ground area year(-1) in a non-fire year, or approximately 13% of the annual gross primary production. We contrasted the canopy physiology of two co-dominant overstory tree species, one of which has a smooth bark on its branches capable of photosynthetic re-fixation (Eucalyptus miniata), and the other of which has a thick, rough bark incapable of re-fixation (Eucalyptus tetrodonta). Eucalyptus miniata supported a larger branch sapwood cross-sectional area in the crown per unit subtending leaf area, and had higher leaf stomatal conductance and photosynthesis than E. tetrodonta. Re-fixation by photosynthetic bark reduces the C cost of delivering water to evaporative sites in leaves, because it reduces the net C cost of constructing and maintaining sapwood. We suggest that re-fixation allowed leaves of E. miniata to photosynthesize at higher rates than those of E. tetrodonta, while the two invested similar amounts of C in the maintenance of branch sapwood. C1 Charles Darwin Univ, Sch Sci & Primary Ind, Fac Educ Hlth & Sci, Darwin, NT 0909, Australia. Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia. RP Cernusak, LA (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Balboa, Panama. EM cernusakl@si.edu RI Cernusak, Lucas/A-6859-2011; Hutley, Lindsay/A-7925-2011; Beringer, Jason/B-8528-2008 OI Cernusak, Lucas/0000-0002-7575-5526; Hutley, Lindsay/0000-0001-5533-9886; Beringer, Jason/0000-0002-4619-8361 NR 81 TC 47 Z9 52 U1 0 U2 18 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD APR PY 2006 VL 29 IS 4 BP 632 EP 646 DI 10.1111/j.1365-3040.2005.01442.x PG 15 WC Plant Sciences SC Plant Sciences GA 027AT UT WOS:000236385900015 PM 17080613 ER PT J AU Kilpatrick, AM Kramer, LD Jones, MJ Marra, PP Daszak, P AF Kilpatrick, AM Kramer, LD Jones, MJ Marra, PP Daszak, P TI West Nile virus epidemics in North America are driven by shifts in mosquito feeding behavior SO PLOS BIOLOGY LA English DT Article ID NEW-YORK-CITY; INFECTIOUS-DISEASES; ENCEPHALITIS-VIRUS; RISK-FACTORS; CULEX; IDENTIFICATION; EMERGENCE; VECTOR; TRANSMISSION; CALIFORNIA AB West Nile virus (WNV) has caused repeated large-scale human epidemics in North America since it was first detected in 1999 and is now the dominant vector-borne disease in this continent. Understanding the factors that determine the intensity of the spillover of this zoonotic pathogen from birds to humans (via mosquitoes) is a prerequisite for predicting and preventing human epidemics. We integrated mosquito feeding behavior with data on the population dynamics and WNV epidemiology of mosquitoes, birds, and humans. We show that Culex pipiens, the dominant enzootic (bird-to-bird) and bridge (bird-to-human) vector of WNV in urbanized areas in the northeast and north-central United States, shifted its feeding preferences from birds to humans by 7-fold during late summer and early fall, coinciding with the dispersal of its preferred host (American robins, Turdus migratorius) and the rise in human WNV infections. We also show that feeding shifts in Cx. tarsalis amplify human WNV epidemics in Colorado and California and occur during periods of robin dispersal and migration. Our results provide a direct explanation for the timing and intensity of human WNV epidemics. Shifts in feeding from competent avian hosts early in an epidemic to incompetent humans after mosquito infection prevalences are high result in synergistic effects that greatly amplify the number of human infections of this and other pathogens. Our results underscore the dramatic effects of vector behavior in driving the transmission of zoonotic pathogens to humans. C1 Consortium Conservat Med, New York, NY USA. New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kilpatrick, AM (reprint author), Consortium Conservat Med, New York, NY USA. EM kilpatrick@conservationmedicine.org FU NIAID NIH HHS [N01AI25490] NR 49 TC 251 Z9 259 U1 8 U2 102 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1544-9173 J9 PLOS BIOL JI PLoS. Biol. PD APR PY 2006 VL 4 IS 4 BP 606 EP 610 AR E82 DI 10.1371/journal.pbio.0040082 PG 5 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 036JD UT WOS:000237066500014 PM 16494532 ER PT J AU Kawahara, AY Adaniski, D AF Kawahara, AY Adaniski, D TI Taxonomic and behavioral studies of a new dancing Beltheca Busck (Lepidoptera : Gelechiidae) from Costa Rica SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Anacampsinae; behavior; Beltheca; Commatica; courtship dance; microlepidoptera; morphology; predator avoidance; taxonomy AB Beltheca oni, new species, is described from the Atlantic lowlands of Costa Rica. The adult female is similar to that of B. picolella Busck, but the former lacks a signum. The male can be distinguished from that of Beltheca phosphoropa (Meyrick) by its longer vinculum and larger aedeagus. Adults of both sexes "dance" on leaves of different plants by anchoring one of their forelegs to a substrate and rotating around this pivot point. The anchored leg shifts slightly when the moth dances in large circles, moves to another region of the leaf, or changes the direction of rotation. There is no preference for rotating clockwise or counterclockwise. Dancing occurs all over the adaxial leaf surface, but it can be localized. An adult was observed dancing around a water droplet and drinking from it. We hypothesize that dancing is a courtship behavior or a predator avoidance tactic. A photograph of the adult and illustrations of the head, wing venation, and genitalia of both sexes are included along with a diagram of a dancing path. C1 Univ Maryland, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Kawahara, AY (reprint author), Univ Maryland, Maryland Ctr Systemat Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. EM kawahara@umd.edu; dadamski@sel.barc.usda.gov NR 14 TC 5 Z9 7 U1 1 U2 2 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 APR PY 2006 VL 108 IS 2 BP 253 EP 260 PG 8 WC Entomology SC Entomology GA 028XX UT WOS:000236523200001 ER PT J AU Neunzig, HH Solis, MA AF Neunzig, HH Solis, MA TI Redescription of Bethulia championella Ragonot (Lepidoptera : Pyralidae : Phycitinae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE phycitinae; southwestern United States; Mexico; Central America; South America AB Based on a single female specimen, Ragonot (1888) described the genus Bethulia and its included species B. championella. Recently, additional specimens of both sexes of this small phycitine have been collected, chiefly in the Neotropics. Using this new material, the genus and species are redescribed, and the male genitalia are illustrated for the first time. C1 N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. Smithsonian Inst, Systemat Entomol Lab, PSI, USDA ARS,Nat Museum Nat Hist, Washington, DC 20013 USA. RP Neunzig, HH (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM asolis@sel.barc.usda.gov NR 4 TC 1 Z9 1 U1 1 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 APR PY 2006 VL 108 IS 2 BP 285 EP 288 PG 4 WC Entomology SC Entomology GA 028XX UT WOS:000236523200005 ER PT J AU LaPolla, JS Longino, JT AF LaPolla, JS Longino, JT TI An unusual new Brachymyrmex Mayr (Hymenoptera : Formicidae) from Costa Rica, with implications for the phylogeny of the Lashne tribe group SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Pseudaphomomyrmex; Myrmelachista; new species; biogeography; Formicinae; Dolichoderinae AB Brachymyrmex Mayr is an exclusively New World ant genus that currently contains 38 described species. In this study, we describe Brachymyrmex nebulosus, new species from Costa Rica. The new species exhibits morphological characters suggestive of both Brachymyrmex and Myrmelachista Roger. Notes on the morphological characters that separate these two genera from each other are provided. Analysis of male genitalia suggests that Brachymyrmex is most closely related to Myrmelachista and Cladomyrma Wheeler, W.M. Previously, the African genera Aphomomyrmex Emery and Petalomyrmex Snelling were thought to be close relatives of Brachymyrmex as well, but our analysis, based on evidence from male genitalia, suggests this is not the case. The monotypic genus Pseudaphomomyrmex Wheeler, W.M, originally placed in the Formicinae and long thought to be a relative of Brachymyrmex, is transferred to the Dolichoderinae. Pseudaphomomyrmex lacks the most obvious synapomorphy of the Formicinae, an acidopore. The species possesses a "dolichoderine habitus." Other morphological characteristics suggest placement within the Dolichoderinae. For instance, the juncture where the mandibular masticatory margin dolichoderines. The structure of the petiole also suggests placement within the subfamily. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. Evergreen State Coll, Olympia, WA 98505 USA. RP LaPolla, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, PO 37012,MRC 188, Washington, DC 20013 USA. EM lapollaj@si.edu; longinoj@evergreen.edu NR 16 TC 5 Z9 6 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 APR PY 2006 VL 108 IS 2 BP 297 EP 305 PG 9 WC Entomology SC Entomology GA 028XX UT WOS:000236523200007 ER PT J AU Adamski, D Brown, JW White, WH AF Adamski, D Brown, JW White, WH TI Description of the immature stages of Pyroderces badia (Hodges) (Lepidoptera : Cosmopterigidae), with a new host record from Louisiana SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Cosmopterigidae; Gelechioidea; scavenger; Sorghum AB The last larval instar and pupa of Pyroderces badia (Hodges) are described and illustrated based on specimens collected from seed heads of sorghum (Sorghum bicolor (L.) Moench) (Poaceae) in southern Louisiana. The species is a well-known scavenger on a wide array of plant material. C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,USDA ARS, Washington, DC 20013 USA. So Reg Res Ctr, Sugarcane Res Unit, Houma, LA 70360 USA. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,USDA ARS, POB 37012,MRC 168, Washington, DC 20013 USA. EM dadamski@sel.barc.usda.gov; jbrown@sel.barc.usda.gov; wwhite@srrc.ars.usda.gov NR 5 TC 3 Z9 4 U1 0 U2 2 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 APR PY 2006 VL 108 IS 2 BP 341 EP 346 PG 6 WC Entomology SC Entomology GA 028XX UT WOS:000236523200011 ER PT J AU Rosolowsky, E Leroy, A AF Rosolowsky, E Leroy, A TI Bias-free measurement of giant molecular cloud properties SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID 1ST GALACTIC QUADRANT; CO SURVEY; OUTER GALAXY; MAGELLANIC-CLOUD; M33; COMPLEXES; MASS AB We review methods for measuring the sizes, line widths, and luminosities of giant molecular clouds (GMCs) in molecular-line data cubes with low resolution and sensitivity. We find that moment methods are robust and sensitive, making full use of both position and intensity information, and we recommend a standard method to measure the position angle, major and minor axis sizes, line width, and luminosity using moment methods. Without corrections for the effects of beam convolution and sensitivity to GMC properties, the resulting properties may be severely biased. This is particularly true for extragalactic observations, where resolution and sensitivity effects often bias measured values by 40% or more. We correct for finite spatial and spectral resolutions with a simple deconvolution, and we correct for sensitivity biases by extrapolating properties of a GMC to those we would expect to measure with perfect sensitivity (i.e., the 0 K isosurface). The resulting method recovers the properties of a GMC to within 10% over a large range of resolutions and sensitivities, provided the clouds are marginally resolved with a peak signal-to-noise ratio greater than 10. We note that interferometers systematically underestimate cloud properties, particularly the flux from a cloud. The degree of bias depends on the sensitivity of the observations and the (u, v) coverage of the observations. In an Appendix to the paper we present a conservative, new decomposition algorithm for identifying GMCs in molecular-line observations. This algorithm treats the data in physical rather than observational units (i.e., parsecs rather than beams or arcseconds), does not produce spurious clouds in the presence of noise, and is sensitive to a range of morphologies. As a result, the output of this decomposition should be directly comparable among disparate data sets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Rosolowsky, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 66, Cambridge, MA 02138 USA. EM erosolow@cfa.harvard.edu; aleroy@astro.berkeley.edu NR 38 TC 83 Z9 83 U1 0 U2 0 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 APR PY 2006 VL 118 IS 842 BP 590 EP 610 DI 10.1086/502982 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 038SW UT WOS:000237247600005 ER PT J AU Vrsnak, B Temmer, M Veronig, A Karlicky, M Lin, J AF Vrsnak, B Temmer, M Veronig, A Karlicky, M Lin, J TI Shrinking and cooling of flare loops in a two-ribbon flare SO SOLAR PHYSICS LA English DT Article ID SOLAR-FLARES; SUPRA-ARCADE; RECONNECTION; MOTIONS; PLASMA; RADIATION; COMPONENT; RIBBONS; MODELS; ORIGIN AB We analyze the evolution of the flare/postflare-loop system in the two-ribbon flare of November 3, 2003, utilizing multi-wavelength observations that cover the temperature range from several tens of MK down to 10(4) K. A non-uniform growth of the loop system enables us to identify analogous patterns in the height - time, h(t), curves measured at different temperatures. The "knees," " plateaus," and " bends" in a higher-temperature curve appear after a certain time delay at lower heights in a lower-temperature curve. We interpret such a shifted replication as a track of a given set of loops ( reconnected field lines) while shrinking and cooling after being released from the reconnection site. Measurements of the height/time shifts between h( t) curves of different temperatures provide a simultaneous estimate of the shrinkage speed and cooling rate in a given temperature domain, for a period of almost ten hours after the flare impulsive phase. From the analysis we find the following: ( a) Loop shrinkage is faster at higher temperatures - in the first hour of the loop-system growth, the shrinkage velocity at 5 MK is 20 - 30 km s(-1), whereas at 1 MK it amounts to 5 km s(-1); (b) Shrinking becomes slower as the flare decays - ten hours after the impulsive phase, the shrinkage velocity at 5 MK becomes 5 km s(-1); ( c) The cooling rate decreases as the flare decays - in the 5 MK range it is 1 MK min(-1) in the first hour of the loop-system growth, whereas ten hours later it decreases to 0.2 MK min(-1); (d) During the initial phase of the loop-system growth, the cooling rate is larger at higher temperatures, whereas in the late phases the cooling rate apparently does not depend on the temperature; ( e) A more detailed analysis of shrinking/cooling around one hour after the impulsive phase reveals a deceleration of the loop shrinkage, amounting to (a) over bar approximate to 10 m s(-2) in the T < 5 MK range; (f) In the same interval, conductive cooling dominates down to T approximate to 3 MK, whereas radiation becomes dominant below T approximate to 2 MK; (g) A few hours after the impulsive phase, radiation becomes dominant across the whole T < 5 MK range. These findings are compared with results of previous studies and discussed in the framework of relevant models. C1 Fac Geodesy, Hvar Observ, Zagreb, Croatia. Graz Univ, Inst Phys, IGAM, Graz, Austria. Acad Sci Czech Republ, Inst Astron, CS-25165 Ondrejov, Czech Republic. Chinese Acad Sci, Yunnan Astron Observ, Kunming, Yunnan, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vrsnak, B (reprint author), Fac Geodesy, Hvar Observ, Zagreb, Croatia. EM bvrsnak@geodet.geof.hr; mat@igam.uni-graz.at; asv@igam.uni-graz.at; karlicky@asu.cas.cz; jlin@ynao.ac.cn RI Veronig, Astrid/B-8422-2009; Karlicky, Marian/G-9023-2014; LIN, JUN/B-9890-2017; OI Temmer, Manuela/0000-0003-4867-7558 NR 54 TC 20 Z9 20 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2006 VL 234 IS 2 BP 273 EP 299 DI 10.1007/s11207-006-0093-6 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 039SD UT WOS:000237326300005 ER PT J AU Applequist, WL Wagner, WL Zimmer, EA Nepokroeff, M AF Applequist, WL Wagner, WL Zimmer, EA Nepokroeff, M TI Molecular evidence resolving the systematic position of Hectorella (Portulacaceae) SO SYSTEMATIC BOTANY LA English DT Article DE Caryophyllales; Hectorella; Hectorellaceae; Lyallia; matkK; ndhF; Portulacaceae ID MATK DNA-SEQUENCES; PHYLOGENETIC RECONSTRUCTION; FLOWERING PLANTS; RBCL SEQUENCES; CARYOPHYLLALES; CENTROSPERMAE; AMARANTHACEAE; LIKELIHOOD; PARSIMONY; ATPB AB The taxonomic position of Hectorella caespitosa and Lyallia kergelensis, caespitose plants endemic to New Zealand and to the Kerguelen Archipelago of Antarctica, respectively, remains controversial. Some authors place them within Portulacaceae, but a slight majority of recent authorities treat them as a separate family, Hectorellaceae. Sequences of the chloroplast genes rbcL, ndhF and matK were obtained from H. caespitosa and added to previously published sequences from Portulacaceae and related families. These data strongly supported the derived position of Hectorella within a clade consisting of western American members of Portulacaceae; the sister group of Hectorella was a clade including Montia, Claytonia, and Lewisia. Implications for taxonomy are discussed. In order to accomodate monophyly in tribal-level classification while preserving current tribes Montieae and Lewiseae, the new tribe Hectorelleae is proposed for the family Portulacaceae. C1 Missouri Bot Garden, William L Brown Ctr Plant Genet Resources, St Louis, MO 63166 USA. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Natl Trop Bot Garden, Kalaheo, HI 96741 USA. Smithsonian Inst, Lab Analyt Biol, Museum Support Ctr, Suitland, MD 20746 USA. Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. RP Applequist, WL (reprint author), Missouri Bot Garden, William L Brown Ctr Plant Genet Resources, Pob 299, St Louis, MO 63166 USA. EM wendy.applequist@mobot.org RI Zimmer, Elizabeth/G-3890-2011 NR 67 TC 20 Z9 21 U1 1 U2 2 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD APR-JUN PY 2006 VL 31 IS 2 BP 310 EP 319 DI 10.1600/036364406777585900 PG 10 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 053CJ UT WOS:000238281000009 ER PT J AU Crouch, TD AF Crouch, TD TI Dr. Space: The life of Wernher von Braun. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, 1000 Jefferson Dr SW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2006 VL 47 IS 2 BP 455 EP 456 DI 10.1353/tech.2006.0117 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 057KS UT WOS:000238595300040 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI First man: The life of Neil A. Armstrong. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, 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 J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2006 VL 47 IS 2 BP 457 EP 458 DI 10.1353/tech.2006.0144 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 057KS UT WOS:000238595300041 ER PT J AU Kidwell, PA AF Kidwell, PA TI Alan Turing's automatic computing engine: The master codebreaker's struggle to build the modern computer. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Div Informat Technol & Commun, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Informat Technol & Commun, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 2 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2006 VL 47 IS 2 BP 460 EP 462 DI 10.1353/tech.2006.0133 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 057KS UT WOS:000238595300043 ER PT J AU Vining, M AF Vining, M TI Grace Hopper: Admiral of the Cyber Sea. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Vining, M (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 J9 TECHNOL CULT JI Technol. Cult. PD APR PY 2006 VL 47 IS 2 BP 462 EP 463 DI 10.1353/tech.2006.0157 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 057KS UT WOS:000238595300044 ER PT J AU Wright, SJ AF Wright, SJ TI Response to Lewis et al.: The uncertain response of tropical forests to global change SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID BIOMASS; PLOTS; DYNAMICS C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 12 TC 10 Z9 10 U1 1 U2 6 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD APR PY 2006 VL 21 IS 4 BP 174 EP 175 DI 10.1016/j.tree.2006.02.003 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 037KB UT WOS:000237144500004 ER PT J AU Agnarsson, I AF Agnarsson, I TI A revision of the New World eximius lineage of Anelosimus (Araneae, Theridiidae) and a phylogenetic analysis using worldwide exemplars SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE evolution of sociality; inbreeding; maternal care; morphology; parallel gains; quasisociality; subsociality; taxonomy; theridiid phylogeny ID WEB-CONSTRUCTION BEHAVIOR; ACHAEARANEA-WAU THERIDIIDAE; EXTRAORDINARY SEX-RATIOS; DIVISION-OF-LABOR; SOCIAL SPIDER; SUBSOCIAL SPIDER; PREY CAPTURE; COOPERATIVE SPIDER; STUDIOSUS ARANEAE; EXPERIMENTAL MANIPULATIONS AB The overwhelming majority of spiders are solitary and territorial. Of the handful of web-sharing social species, most belong to the cobweb genus Anelosimus Simon, 1891 (Theridiidae). Anelosimus species, especially those from the Americas, have therefore become model organisms in the study of spider sociality. However, lack of a phylogeny and outdated taxonomy have hindered progress in understanding the evolution of social behaviour. The identity of many species studied behaviourally is in doubt, and choice among the competing hypotheses on the course of evolution of sociality in Anelosimus requires a robust phylogeny. This paper offers a revision of the New World 'eximius lineage' containing the most intensely studied Anelosimus species, and a phylogenetic study including worldwide exemplars. Previous taxonomic work on the group was incomplete and oversimplified. Some species-level taxa, e.g. A. jucundus (O. P.-Cambridge, 1896) and A. studiosus (Hentz, 1850), as previously circumscribed represent a compendium of species and are here re-examined. Eight new species are here described: A. arizona, A. baeza, A. octavius and A. puravida, of the 'jucundus group', and A. gucamayos, A. oritoyacu, A. pantanal and A. tungurahua of the 'studiosus group'. Furthermore, Enoplognatha dubia Chamberlin, 1916 and Theridion tosum Chamberlin, 1916 previously synonymized with A. jucundus, and Anelosimus fraternus Bryant, 1948, previously synonymized with A. studiosus, are here again considered valid. Enoplognatha dubia becomes a junior secondary homonym of Brattia dubia Tullgren, 1910 (= Anelosimus dubius) and the replacement name Anelosimus elegans Nomen Novum is here provided. The parsimony analysis of the morphological matrix (43 taxa, 147 characters) resulted in two equally most parsimonious trees, with four trichotomies in the strict consensus. Three of these lack character evidence to resolve them; one is a result of character conflict. One of the two trees is optimal under successive weighting. The New World Anelosimus are not monophyletic, but rather form three clades, the eximius lineage (20 species), the 'rupununi group' (two species) and the 'ethicus group' (six species). The phylogenetic results corroborate previous transfer of species to Kochiura and Selkirkiella. The following additional species are removed from Anelosimus: Styposis camoteensis (Levi, 1967) (comb. nov.), Styposis tepus (Levi, 1967) (comb. nov.), Chrosiothes episinoides (Levi, 1963) (comb. nov.) and Stemmops osorno (Levi, 1963) (comb. nov.). Four species are here treated as nomina dubia, Anelosimus nigrobaricus Barrion & Litsinger, 1995 (type in very bad condition, original description lacks sufficient detail for identification), and A. salaensis Barrion & Litsinger, 1995, Theridion fasciatum Holmberg, 1876 and T. sordidum Holmberg, 1876 (types lost, original descriptions lacks sufficient detail for identification). The results corroborate previous findings of convergent evolution of permanent sociality in the genus. However, instead of sociality evolving twice as previously suspected, the current phylogeny suggests no less than six, independent origins. Each time, the evolution of sociality seems to be responsible for a dramatic shift in population structure from outbred panmictic to strongly inbred subdivided populations. Perhaps as a consequence, once they are permanently social, species seem to fail to diversify; all social clades are small (one or two species) and usually smaller than their sister clade. No losses of social behaviour are inferred. The maternal care routehypothesis is again supported. To explain sociality in Anelosimus it seems sufficient to hypothesize a temporal extension of the juvenile web-sharing, co-operation and conspecific tolerance, displayed in basic maternal care, coupled with depression of dispersal. Given the most parsimonious phylogeny, the basal-most Anelosimus species occur in the Old World, and three Anelosimus clades occur in the New World. Sufficient data are not available to estimate the age of the Anelosimus lineage accurately, but the sparse fossil record hints at a relatively recent origin (20-40 mya). If true, vicariance could not account for this distribution; rather, the pattern may suggest three independent colonization events of Old World Anelosimus in the Americas. Support for most branches within Anelosimus is relatively low, especially the support for the relationships within species groups. Thus, although the forgoing conclusions are clearly implied by the phylogeny, weak support limits their force. (C) 2006 The Linnean Society of London. C1 Smithsonian Inst, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Agnarsson, I (reprint author), Univ British Columbia, Dept Zool, 3529-6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM ingi@zoology.ubc.ca NR 264 TC 68 Z9 70 U1 0 U2 22 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 APR PY 2006 VL 146 IS 4 BP 453 EP 593 DI 10.1111/j.1096-3642.2006.00213.x PG 141 WC Zoology SC Zoology GA 027EO UT WOS:000236396800001 ER PT J AU Grindlay, JE AF Grindlay, JE TI Astronomy - A neutron star in F-sharp SO SCIENCE LA English DT Editorial Material ID MILLISECOND PULSAR; BINARIES AB Discovery of the fastest spinning pulsar gives new constraints on the size of a neutron star and matter under extreme conditions and decreases the need for gravitational waves to impose a limiting maximum spin. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@cfa.harvard.edu NR 13 TC 4 Z9 4 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 MAR 31 PY 2006 VL 311 IS 5769 BP 1876 EP 1877 DI 10.1126/science.1125125 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 027BD UT WOS:000236387800032 PM 16574857 ER PT J AU Jaramillo, C Rueda, MJ Mora, G AF Jaramillo, C Rueda, MJ Mora, G TI Cenozoic plant diversity in the Neotropics SO SCIENCE LA English DT Article ID RAIN-FOREST; EASTERN CORDILLERA; SOUTH-AMERICA; CLIMATE; VEGETATION; TERTIARY; BASIN; DIVERSIFICATION; BIODIVERSITY; PLEISTOCENE AB Several mechanisms have been proposed to explain the high levels of plant diversity in the Neotropics today, but little is known about diversification patterns of Neotropical floras through geological time. Here, we present the longest time series compiled for palynological plant diversity of the Neotropics (15 stratigraphic sections, 1530 samples, 1411 morphospecies, and 287,736 occurrences) from the Paleocene to the early Miocene (65 to 20 million years ago) in central Colombia and western Venezuela. The record shows a low-diversity Paleocene flora, a significantly more diverse early to middle Eocene flora exceeding Holocene levels, and a decline in diversity at the end of the Eocene and early Oligocene. A good correlation between diversity fluctuations and changes in global temperature was found, suggesting that tropical climate change may be directly driving the observed diversity pattern. Alternatively, the good correspondence may result from the control that climate exerts on the area available for tropical plants to grow. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Unit 0948, APO, AA 34002 USA. Paleoflora Colombian Petr Inst, Bucaramanga, Colombia. Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA 50011 USA. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Unit 0948, APO, AA 34002 USA. EM jaramilloc@si.edu NR 44 TC 173 Z9 186 U1 6 U2 57 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 MAR 31 PY 2006 VL 311 IS 5769 BP 1893 EP 1896 DI 10.1126/science.1121380 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 027BD UT WOS:000236387800036 PM 16574860 ER PT J AU Mitrovica, JX Wahr, J Matsuyama, I Paulson, A Tamisiea, ME AF Mitrovica, JX Wahr, J Matsuyama, I Paulson, A Tamisiea, ME TI Reanalysis of ancient eclipse, astronomic and geodetic data: A possible route to resolving the enigma of global sea-level rise SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE ancient eclipses; polar wander; Earth rotation; global sea level; glacial rebound ID EARTHS ROTATION AXIS; PLEISTOCENE DEGLACIATION; MANTLE; FLUCTUATIONS; MODEL; FIELD AB Predictions of the Earth's response to the ice age appear to simultaneously reconcile a set of astronomical, geodetic and ancient eclipse observations related to changes in rotation, thus ruling out ice melting as a major contributor to 20th century sea-level rise. We demonstrate that the reconciliation disappears when an improved theory of rotational stability is applied. Furthermore, our reanalysis of longer satellite records renders previous estimates of the secular change in rotation rate suspect. The updated ice-age predictions and observations permit an anomalous 20th century ice flux of similar to 1 mm/yr equivalent sea-level rise. Thus, the full suite of Earth rotation observations are consistent with a connection between climatic warming and recent melting of ice reservoirs. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. Univ Colorado, CIRES, Boulder, CO 80309 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mitrovica, JX (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM jxm@physics.utoronto.ca OI Matsuyama, Isamu/0000-0002-2917-8633 NR 50 TC 34 Z9 35 U1 2 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 MAR 30 PY 2006 VL 243 IS 3-4 BP 390 EP 399 DI 10.1016/j.epsl.2005.12.029 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 029YP UT WOS:000236600600008 ER PT J AU Gaudin, TJ Emry, RJ Pogue, B AF Gaudin, TJ Emry, RJ Pogue, B TI A new genus and species of pangolin (Mammalia, Pholidota) from the late Eocene of Inner Mongolia, China SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID POSTCRANIAL SKELETON; GIANT PANGOLIN AB A partial postcranial skeleton from the late Eocene of the Shara Murun region of northern China is described as a new genus and species of fossil pangolin, Cryptomanis gobiensis. Cryptomanis displays numerous diagnostic pangolin characteristics, including enrolled lumbar zygapophyses and fissured ungual phalanges. Like the anatomically similar North American Eocene pangolin Patriomanis, it retains primitive mammalian features such as a convex astragalar head and a prominent femoral third trochanter that are lost in extant pangolins. The systematic position of Cryptonmanis within Pholidota is not unambiguously resolved. It is tentatively placed in the family Patriomanidae, which we restrict to Cryptomanis and the closely similar Patriomanis. Cryptomanis differs from modern pangolins in its more robust proximal limb elements, its lack of a greatly enlarged third manual digit, its slender tail, and its more elongate, grasping pedal digits. These traits suggest an animal well adapted for digging but with a tendency toward a semi-arboreal lifestyle. This new genus and species represents the oldest and most northerly Asian record of pangolins, and indicates that pangolins were widely distributed throughout Laurasia during the Eocene. It is consistent with a Laurasian origin for pangolins. C1 Univ Tennessee, Dept Biol & Environm Sci, Chattanooga, TN 37403 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Gaudin, TJ (reprint author), Univ Tennessee, Dept Biol & Environm Sci, 615 McCallie Ave, Chattanooga, TN 37403 USA. EM Timothy-Gaudin@utc.edu; emryr@si.edu NR 48 TC 7 Z9 7 U1 2 U2 4 PU SOC VERTEBRATE PALEONTOLOGY PI NORTHBROOK PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAR 30 PY 2006 VL 26 IS 1 BP 146 EP 159 DI 10.1671/0272-4634(2006)26[146:ANGASO]2.0.CO;2 PG 14 WC Paleontology SC Paleontology GA 030FB UT WOS:000236618500015 ER PT J AU Nearns, EH Steiner, WE AF Nearns, EH Steiner, WE TI A new species of Plectromerus Haldeman (Coleoptera : Cerambycidae) from Navassa Island, Greater Antilles SO ZOOTAXA LA English DT Article DE Cerambycinae; Curiini; Caribbean; West Indies; taxonomy; endemic AB A new species, Plectromerus navassae (Coleoptera: Cerambycidae: Cerambycinae: Curiini), from Navassa Island, Greater Antilles, is described. Features distinguishing the new species from its congeners are presented. C1 Univ Florida, Dept Entomol & Nematol, Gainesville, FL 32611 USA. Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Nearns, EH (reprint author), Univ Florida, Dept Entomol & Nematol, Gainesville, FL 32611 USA. EM gnearns@ufl.edu; steinerw@si.edu NR 14 TC 3 Z9 4 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 MAR 30 PY 2006 IS 1163 BP 61 EP 68 PG 8 WC Zoology SC Zoology GA 026TD UT WOS:000236364300003 ER PT J AU Cole, C Winter, J AF Cole, Christina Winter, John TI Identification of organic red dyes on late Qing dynasty ancestor portraits via HPLC and GC/MS SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 231st National Meeting of the American-Chemical-Society CY MAR 26-30, 2006 CL Atlanta, GA SP Amer Chem Soc C1 Smithsonian Inst, Freer Gallery Art, Washington, DC 20560 USA. Arthur M Sackler Gallery, Washington, DC 20560 USA. EM colecl@asia.si.edu 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 MAR 26 PY 2006 VL 231 MA 412-ANYL PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA 050YE UT WOS:000238125900519 ER PT J AU Melnick, GJ AF Melnick, Gary J. TI Water, molecular oxygen, and the chemical structure of molecular clouds SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 231st National Meeting of the American-Chemical-Society CY MAR 26-30, 2006 CL Atlanta, GA SP Amer Chem Soc C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM gmelnick@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 0 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 MAR 26 PY 2006 VL 231 MA 492-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 050YE UT WOS:000238125908610 ER PT J AU Steiner, WE AF Steiner, WE TI New species of darkling beetles (Coleoptera : Tenebrionidae) from San Salvador Island, Bahamas SO ZOOTAXA LA English DT Article DE Bahamas; beach insects; darkling beetles; images of holotypes; island endemism; maritime scrub; new species; San Salvador Island; Tenebrionidae ID BRANCHUS; ADELINA AB In preparation for a survey and annotated checklist of the Tenebrionidae of San Salvador Island, Bahamas, nine new species of darkling beetles are described. All are so far known only from this island and probably endemic. The majority of them are flightless. All inhabit maritime sand scrub habitats. The new taxa, in the sequence described herein, are: Trientoma jilae, n. sp., Trientoma voegeliorum, n. sp., Branchus geraceorum, n. sp., Adelina bacardi, n. sp., Blapstinus kalik, n. sp., Diastolinus this, n. sp., Diastolinus that, n. sp., Nautes guanahani, n. sp., Lobopoda deyrupi, n. sp. Digital images of the holotypes are included. Diagnoses of the new species, with comparisons among related ones, are provided, and notes on habitats and collections are given. One species, Blapstinus humilis Casey, is brought out of synonymy under B. fuscus Casey and provisionally recognized as valid, pending further revisionary work. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Dept Entomol, NHB-187, Washington, DC 20560 USA. NR 21 TC 3 Z9 3 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 MAR 23 PY 2006 IS 1158 BP 1 EP 38 PG 38 WC Zoology SC Zoology GA 024IN UT WOS:000236188800001 ER PT J AU Little, AEF Murakami, T Mueller, UG Currie, CR AF Little, Ainslie E. F. Murakami, Takahiro Mueller, Ulrich G. Currie, Cameron R. TI Defending against parasites: fungus-growing ants combine specialized behaviours and microbial symbionts to protect their fungus gardens SO BIOLOGY LETTERS LA English DT Article DE actinomycete; behavioural ecology; Escovopsis; host-parasite interaction; mutualism; pathogen ID OCTOSPINOSUS REICH HYMENOPTERA; FORMICIDAE; BACTERIA; POCKET AB Parasites influence host biology and population structure, and thus shape the evolution of their hosts. Parasites often accelerate the evolution of host defences, including direct defences such as evasion and sanitation and indirect defences such as the management of beneficial microbes that aid in the suppression or removal of pathogens. Fungus-growing ants are doubly burdened by parasites, needing to protect their crops as well as themselves from infection. We show that parasite removal from fungus gardens is more complex than previously realized. In response to infection of their fungal gardens by a specialized virulent parasite, ants gather and compress parasitic spores and hyphae in their infrabuccal pockets, then deposit the resulting pellet in piles near their gardens. We reveal that the ants' infrabuccal pocket functions as a specialized sterilization device, killing spores of the garden parasite Escovopsis. This is apparently achieved through a symbiotic association with actinomycetous bacteria in the infrabuccal pocket that produce antibiotics which inhibit Escovopsis. The use of the infrabuccal pocket as a receptacle to sequester Escovopsis, and as a location for antibiotic administration by the ants' bacterial mutualist, illustrates how the combination of behaviour and microbial symbionts can be a successful defence strategy for hosts. C1 Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Trop Res Inst, Ancona, Italy. Hokkaido Univ, Fac Sci, Chromosome Res Unit, Sapporo, Hokkaido 0600810, Japan. Univ Texas, Patterson Labs, Sect Integrat Biol, Austin, TX 78712 USA. RP Little, AEF (reprint author), Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM alittle@wisc.edu NR 21 TC 55 Z9 57 U1 2 U2 20 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETT-UK JI Biol. Lett. PD MAR 22 PY 2006 VL 2 IS 1 BP 12 EP 16 DI 10.1098/rsbl.2005.0371 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 104KV UT WOS:000241958200004 PM 17148313 ER PT J AU Collins, AG Bentlage, B Matsumoto, GI Haddock, SHD Osborn, KJ Schierwater, B AF Collins, Allen G. Bentlage, Bastian Matsumoto, George I. Haddock, Steven H. D. Osborn, Karen J. Schierwater, Bernd TI Solution to the phylogenetic enigma of Tetraplatia, a worm-shaped cnidarian SO BIOLOGY LETTERS LA English DT Article DE Scyphozoa; Coronatae; Hydrozoa; Narcomedusae; ribosomal DNA; bodyplan evolution ID TREE SELECTION; MEDUSOZOA; EVOLUTION AB Tetraplatia is a genus containing two species of pelagic cnidarians of curious morphology. Their vermiform shape and four swimming flaps are difficult to relate to the features of other cnidarians, thus obscuring their phylogenetic affinities. Since their discovery in the mid-1800s, a number of prominent cnidarian workers have weighed in on this conundrum, some arguing that they are aberrant hydrozoans and others concluding that they are unusual scyphozoans. Current taxonomic practice conforms to the latter view. However, data presented here from the large and small subunits of the nuclear ribosome leave little doubt that Tetraplatia is in fact a hydrozoan genus. Indeed, its precise phylogenetic position is within Narcomedusae, as some authors had previously deduced based on structural characters. The distinctive body plan of Tetraplatia is remarkable because it appears to have a recent origin, in contrast to the prevailing pattern of metazoan history. C1 Smithsonian Inst, NMFS, Natl Systemat Lab, Natl Museum Nat Hist,MRC 153, Washington, DC 20013 USA. Univ Gottingen, Ctr Biodivers & Ecol, D-37077 Gottingen, Germany. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. TiHo Hannover, ITZ, D-30559 Hannover, Germany. RP Collins, AG (reprint author), Smithsonian Inst, NMFS, Natl Systemat Lab, Natl Museum Nat Hist,MRC 153, POB 37012, Washington, DC 20013 USA. EM collinsa@si.edu RI Collins, Allen/A-7944-2008; Osborn, Karen/E-9222-2011; OI Collins, Allen/0000-0002-3664-9691; Osborn, Karen/0000-0002-4226-9257 NR 31 TC 9 Z9 10 U1 0 U2 1 PU ROYAL SOCIETY PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETT-UK JI Biol. Lett. PD MAR 22 PY 2006 VL 2 IS 1 BP 120 EP 124 DI 10.1098/rsbl.2005.0372 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 104KV UT WOS:000241958200034 PM 17148343 ER PT J AU Fender, RP Muxlow, TWB Garrett, MA Kouveliotou, C Gaensler, BM Garrington, ST Paragi, Z Tudose, V Miller-Jones, JCA Spencer, RE AF Fender, RP Muxlow, TWB Garrett, MA Kouveliotou, C Gaensler, BM Garrington, ST Paragi, Z Tudose, V Miller-Jones, JCA Spencer, RE TI Structure in the radio counterpart to the 2004 December 27 giant flare from SGR 1806-20 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars : individual : SGR1806-20; ISM : jets and outflows; radio continuum : stars ID MAGNETAR SGR-1806-20; DISTANCE; PULSAR; NEBULA; JETS AB On 2004 December 27, the magnetar SGR 1806-20 underwent an enormous outburst resulting in the formation of an expanding, moving, and fading radio source. We report observations of this radio source with the Multi-Element Radio-Linked Interferometer Network and the Very Long Baseline Array. The observations confirm the elongation and expansion already reported based on observations at lower angular resolutions, but suggest that at early epochs the structure is not consistent with the very simplest models such as a smooth flux distribution. In particular, there appears to be significant structure on small angular scales, with similar to 10 per cent of the radio flux arising on angular scales <= 100 milliarcsec. This structure may correspond to localized sites of particle acceleration during the early phases of expansion and interaction with the ambient medium. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Romanian Acad, Inst Astron, RO-040557 Bucharest, Romania. Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Fender, RP (reprint author), Univ Southampton, Sch Phys & Astron, Highfield, Southampton SO17 1BJ, Hants, England. EM rpf@phys.soton.ac.uk RI Gaensler, Bryan/F-8655-2010; Tudose, Valeriu/F-8976-2010; Miller-Jones, James/B-2411-2013; OI Miller-Jones, James/0000-0003-3124-2814; Muxlow, Thomas/0000-0001-5797-8796; Wijers, Ralph/0000-0002-3101-1808; Gaensler, Bryan/0000-0002-3382-9558 NR 23 TC 8 Z9 8 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2006 VL 367 IS 1 BP L6 EP L10 DI 10.1111/j.1745-3933.2006.00123.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 020VA UT WOS:000235939700002 ER PT J AU Babich, D Loeb, A AF Babich, D Loeb, A TI Imprint of inhomogeneous reionization on the power spectrum of galaxy surveys at high redshifts SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation ID DARK-MATTER HALOES; PROBE WMAP OBSERVATIONS; LY-ALPHA FOREST; INTERGALACTIC MEDIUM; COSMOLOGICAL REIONIZATION; FLUCTUATIONS; HYDROGEN; CONDENSATION; STATISTICS; CLUSTERS AB We consider the effects of inhomogeneous reionization on the distribution of galaxies at high redshifts. Modulation of the formation process of the ionizing sources by large-scale density modes makes reionization inhomogeneous and introduces a spread to the reionization times of different regions with the same size. After sources photoionize and heat these regions to a temperature >= 10(4) K at different times, their temperatures evolve as the ionized intergalactic medium (IGM) expands. The varying IGM temperature makes the minimum mass of galaxies spatially nonuniform with a fluctuation amplitude that increases toward small scales. These scale-dependent fluctuations modify the shape of the power spectrum of low-mass galaxies at high redshifts in a way that depends on the history of reionization. The resulting distortion of the primordial power spectrum is significantly larger than changes associated with uncertainties in the inflationary parameters, such as the spectral index of the scalar power spectrum or the running of the spectral index. Future surveys of high-redshift galaxies will offer a new probe of the thermal history of the IGM but might have a more limited scope in constraining inflation. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. RP Babich, D (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM babich@physics.harvard.edu; aloeb@cfa.harvard.edu NR 37 TC 18 Z9 18 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP 1 EP 7 DI 10.1086/499942 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100001 ER PT J AU Kochanek, CS Morgan, ND Falco, EE McLeod, BA Winn, JN Dembicky, J Ketzeback, B AF Kochanek, CS Morgan, ND Falco, EE McLeod, BA Winn, JN Dembicky, J Ketzeback, B TI The time delays of gravitational lens HE 0435-1223: An early-type galaxy with a rising rotation curve SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; dark matter; galaxies : kinematics and dynamics; gravitational lensing; quasars : individual (HE 0435-1223) ID DARK-MATTER HALOS; ELLIPTIC GALAXIES; HUBBLE CONSTANT; FIELD GALAXIES; QUADRUPLE QSO; LIGHT CURVES; EVOLUTION; QUASAR; MODELS; SUBSTRUCTURE AB `We present Hubble Space Telescope images and 2 years of optical photometry of the quadruple quasar HE 0435-1223. The time delays between the intrinsic quasar variations are Delta t(AD) = -14.37(-0.85)(+0.75), Delta t(AB)= -8.00(-0.82)(+0.73), and Delta t(AC) = 2.10(-0.71)(+0.78) days. We also observed nonintrinsic variations of similar to 0.1 mag yr(-1) that we attribute to microlensing. Instead of the traditional approach of assuming a rotation curve for the lens galaxy and then deriving the Hubble constant (H-0), we assume H-0 ( 72 +/- 7) km s(-1) Mpc(-1) and derive constraints on the rotation curve. On the scale over which the lensed images occur (1."2 = 5 h(-1) kpc similar or equal to 1.5R(e)), the lens galaxy must have a rising rotation curve, and it cannot have a constant mass- to- light ratio. These results add to the evidence that the structures of earlytype galaxies are heterogeneous. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Apache Point Observ, Sunspot, NM 88349 USA. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. NR 49 TC 97 Z9 97 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 MAR 20 PY 2006 VL 640 IS 1 BP 47 EP 61 DI 10.1086/499766 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100007 ER PT J AU Soria, R Fabbiano, G Graham, AW Baldi, A Elvis, M Jerjen, H Pellegrini, S Siemiginowska, A AF Soria, R Fabbiano, G Graham, AW Baldi, A Elvis, M Jerjen, H Pellegrini, S Siemiginowska, A TI Accretion and nuclear activity of quiescent supermassive black holes. I. X-ray study SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; galaxies : individual (NGC 821, NGC 3377, NGC 4486B, NGC 4564, NGC 4697, NGC 5845); galaxies : nuclei; galaxies : structure; X-rays : galaxies ID EARLY-TYPE GALAXIES; SAGITTARIUS-A-ASTERISK; BONDI-HOYLE ACCRETION; DWARF ELLIPTIC GALAXY; CHANDRA OBSERVATIONS; GALACTIC NUCLEI; DIFFUSE GAS; CENTRAL REGIONS; COOLING FLOWS; ENERGY-DISTRIBUTIONS AB We have studied the nuclear activity in a sample of six quiescent early-type galaxies, with new Chandra data and archival HST optical images. Their nuclear sources have X-ray luminosities similar to 10(38)-10(39) ergs s(-1) (L-X/L-Edd similar to 10(-8) to 10(-7)) and colors or spectra consistent with accreting supermassive black holes ( SMBHs), except for the nucleus of NGC 4486B, which is softer than typical AGN spectra. In a few cases, the X-ray morphology of the nuclear sources shows hints of marginally extended structures, in addition to the surrounding diffuse thermal emission from hot gas, which is detectable on scales greater than or similar to 1 kpc. In one case ( NGC 5845), a dusty disk may partially obstruct our direct view of the SMBH. We have estimated the temperature and density of the hot interstellar medium, which is one major source of fuel for the accreting SMBH; typical central densities are n(e) approximate to (0.02 +/- 0.01) cm(-3). Assuming that the hot gas is captured by the SMBH at the Bondi rate, we show that the observed X-ray luminosities are too faint to be consistent with standard disk accretion, but brighter than predicted by radiatively inefficient solutions ( e. g., advection-dominated accretion flows [ADAFs]). In total, there are approximate to 20 galaxies for which SMBH mass, hot gas density, and nuclear X-ray luminosity are simultaneously known. In some cases, the nuclear sources are brighter than predicted by the ADAF model; in other cases, they are consistent or fainter. We discuss the apparent lack of correlations between Bondi rate and X-ray luminosity and suggest that, in order to understand the observed distribution, we need to know two additional parameters: the amount of gas supplied by the stellar population inside the accretion radius, and the fraction (possibly << 1) of the total gas available that is accreted by the SMBH. We leave a detailed study of these issues to a subsequent paper. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 72611, Australia. Univ Bologna, Dipartmento Astron, I-40127 Bologna, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Graham, Alister/G-1217-2013 OI Graham, Alister/0000-0002-6496-9414 NR 103 TC 45 Z9 45 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 MAR 20 PY 2006 VL 640 IS 1 BP 126 EP 142 DI 10.1086/499934 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100013 ER PT J AU Soria, R Graham, AW Fabbiano, G Baldi, A Elvis, M Jerjen, H Pellegrini, S Siemiginowska, A AF Soria, R Graham, AW Fabbiano, G Baldi, A Elvis, M Jerjen, H Pellegrini, S Siemiginowska, A TI Accretion and nuclear activity of quiescent supermassive black holes. II. Optical study and interpretation SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies : individual (NGC 821, NGC 3377, NGC 4486B, NGC 4564, NGC 4697, NGC 5845); galaxies : nuclei; galaxies : structure; X-rays : galaxies ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; X-RAY BINARIES; MASSIVE ELLIPTIC GALAXIES; JET-DISK SYMBIOSIS; GALACTIC NUCLEI; COOLING FLOWS; STRUCTURAL PARAMETERS; ENERGY-DISTRIBUTIONS; CHANDRA OBSERVATIONS AB Our X-ray study of the nuclear activity in a new sample of six quiescent early-type galaxies, as well as in a larger sample from the literature, confirmed ( Paper I) that the Bondi accretion rate of diffuse hot gas is not a good indicator of the SMBH X-ray luminosity. Here we suggest that a more reliable estimate of the accretion rate must include the gas released by the stellar population inside the sphere of influence of the SMBH, in addition to the Bondi inflow of hot gas across that surface. We use optical surface brightness profiles to estimate the mass-loss rate from stars in the nuclear region: we show that for our sample of galaxies it is an order of magnitude higher (similar to 10(-4) to 10(-3) M-circle dot yr(-1)) than the Bondi inflow rate of hot gas, as estimated from Chandra (Paper I). Only by taking into account both sources of fuel can we constrain the true accretion rate, the accretion efficiency, and the power budget. Radiatively efficient accretion is ruled out, for quiescent SMBHs. For typical radiatively inefficient flows, the observed X-ray luminosities of the SMBHs imply accretion fractions similar to 1%-10% (i.e., similar to 90%-99% of the available gas does not reach the SMBH) for at least five of our six target galaxies and most of the other galaxies with known SMBH masses. We discuss the conditions for mass conservation inside the sphere of influence, so that the total gas injection is balanced by accretion plus outflows. We show that a fraction of the total accretion power (mechanical plus radiative) would be sufficient to sustain a self-regulating, slow outflow that removes from the nuclear region all the gas that does not sink into the BH ("BH feedback''). The rest of the accretion power may be carried out in a jet or advected. We also discuss scenarios that would lead to an intermittent nuclear activity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 72611, Australia. Univ Bologna, Dipartmento Astron, I-40127 Bologna, Italy. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Graham, Alister/G-1217-2013 OI Graham, Alister/0000-0002-6496-9414 NR 86 TC 44 Z9 44 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 MAR 20 PY 2006 VL 640 IS 1 BP 143 EP 155 DI 10.1086/499935 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100014 ER PT J AU Alonso-Herrero, A Perez-Gonzalez, PG Alexander, DM Rieke, GH Rigopoulou, D Le Floc'h, E Barmby, P Papovich, C Rigby, JR Bauer, FE Brandt, WN Egami, E Willner, SP Dole, H Huang, JS AF Alonso-Herrero, A Perez-Gonzalez, PG Alexander, DM Rieke, GH Rigopoulou, D Le Floc'h, E Barmby, P Papovich, C Rigby, JR Bauer, FE Brandt, WN Egami, E Willner, SP Dole, H Huang, JS TI Infrared power-law galaxies in the Chandra deep field-south: Active galactic nuclei and ultraluminous infrared galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : high-redshift; infrared : galaxies; X-rays : galaxies ID X-RAY SOURCES; SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; TYPE-1 SEYFERT-GALAXIES; ARRAY CAMERA IRAC; OPTICAL SPECTROSCOPY; LOCKMAN HOLE; NORTH SURVEY AB We investigate the nature of a sample of 92 Spitzer MIPS 24 mu m-selected galaxies in the CDF-S, showing power-law-like emission in the Spitzer IRAC 3.6-8 mu m bands. The main goal is to determine whether the galaxies not detected in X-rays (47% of the sample) are part of the hypothetical population of obscured AGNs not detected even in deep X-ray surveys. The majority of the IR power-law galaxies are ULIRGs at z > 1, and those with LIRG-like IR luminosities are usually detected in X-rays. The optical-to-IR SEDs of the X-ray-detected galaxies are almost equally divided between a BLAGN SED class (similar to an optically selected QSO) and an NLAGN SED ( similar to the BLAGN SED but with an obscured UV/optical continuum). A small fraction of SEDs resemble warm ULIRGs (e. g., Mrk 231). Most galaxies not detected in X-rays have SEDs in the NLAGN+ULIRG class as they tend to be optically fainter and possibly more obscured. Moreover, the IR power-law galaxies have SEDs significantly different from those of high-z (zsp > 1) IR (24 mu m) selected and optically bright (VVDS I-AB <= 24) star-forming galaxies whose SEDs show a very prominent stellar bump at 1.6 mu m. The galaxies detected in X-rays have 2-8 keV rest- frame luminosities typical of AGNs. The galaxies not detected in X-rays have global X-ray-to-mid-IR SED properties that make them good candidates to contain IR-bright X-ray-absorbed AGNs. If all these sources are actually obscured AGNs, we would observe a ratio of obscured to unobscured 24 mu m-detected AGNs of 2.1, whereas models predict a ratio of up to 3:1. Additional studies using Spitzer to detect X-ray-quiet AGNs are likely to find more such obscured sources. C1 CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, Pupin Labs, New York, NY 10027 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Inst Astrophys Spatiale, F-91405 Orsay, France. RP Alonso-Herrero, A (reprint author), CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, Plaza Murillo 2, E-28006 Madrid, Spain. EM aalonso@damir.iem.csic.es RI Rigby, Jane/D-4588-2012; Brandt, William/N-2844-2015; Barmby, Pauline/I-7194-2016; Perez-Gonzalez, Pablo/J-2871-2016; Alonso-Herrero, Almudena/H-1426-2015; OI Rigby, Jane/0000-0002-7627-6551; Brandt, William/0000-0002-0167-2453; Barmby, Pauline/0000-0003-2767-0090; Perez-Gonzalez, Pablo/0000-0003-4528-5639; Alonso-Herrero, Almudena/0000-0001-6794-2519; Alexander, David/0000-0002-5896-6313 NR 85 TC 183 Z9 183 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP 167 EP 184 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100016 ER PT J AU Harris, DE Cheung, CC Biretta, JA Sparks, WB Junor, W Perlman, ES Wilson, AS AF Harris, DE Cheung, CC Biretta, JA Sparks, WB Junor, W Perlman, ES Wilson, AS TI The outburst of HST-1 in the M87 jet SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (M87); galaxies : jets; X-rays : general ID X-RAY-EMISSION AB The X-ray intensity of knot HST-1, 0."85 from the nucleus of the radio galaxy M87, has increased by more than a factor of 50 during the last 5 yr. The optical increase is similar, and our more limited radio data indicate a commensurate activity. We give the primary results of our Chandra X- Ray Observatory monitoring program and consider some of the implications of this extreme variability in a relativistic jet. We find that the data support a ''modest beaming synchrotron'' model as indicated in our earlier papers. Based on this model, the decay of the X- ray light curve appears to be dominated by the light-travel time across the emitting region of HST-1, rather than synchrotron loss timescales. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM harris@cfa.harvard.edu NR 14 TC 92 Z9 92 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP 211 EP 218 DI 10.1086/500081 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100020 ER PT J AU Maughan, BJ Ellis, SC Jones, LR Mason, KO Cordova, FA Priedhorsky, W AF Maughan, BJ Ellis, SC Jones, LR Mason, KO Cordova, FA Priedhorsky, W TI XMM-Newton observes Cl J0152.7-1357: A massive galaxy cluster forming at merger crossroads at z=0.83 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : clusters : general; galaxies : clusters : individual (Cl J0152.7-1357); galaxies : high-redshift; intergalactic medium; X-rays : galaxies ID LARGE-SCALE FILAMENT; X-RAY-CLUSTERS; CHANDRA OBSERVATION; EVOLUTION; DISCOVERY; ABELL-85; VIEW AB We present an analysis of a 50 ks XMM- Newton observation of the merging galaxy cluster Cl J0152.7 similar to 1357 at z = 0: 83. In addition to the two main subclusters and an infalling group detected in an earlier Chandra observation of the system, XMM- Newton detects another group of galaxies possibly associated with the cluster. This group may be connected to the northern subcluster by a filament of cool ( 1: 4 (+0.3)(-0.1) keV) X- ray-emitting gas and lies outside the estimated virial radius of the northern subcluster. The X- ray morphology agrees well with the projected galaxy distribution in new K-band imaging data presented herein. We use detailed spectral and imaging analysis of the X- ray data to probe the dynamics of the system and find evidence that another subcluster or group has recently passed through the northern subcluster. Cl J0152.7 - 1357 is an extremely dynamically active system, with mergers at different stages occurring along two perpendicular merger axes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. Anglo Australian Observ, Epping, NSW 2121, Australia. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Calif Riverside, Riverside, CA 92521 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. EM bmaughan@cfa.harvard.edu OI Priedhorsky, William/0000-0003-0295-9138 NR 38 TC 18 Z9 18 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 MAR 20 PY 2006 VL 640 IS 1 BP 219 EP 227 DI 10.1086/499939 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100021 ER PT J AU Marrone, DP Moran, JM Zhao, JH Rao, R AF Marrone, DP Moran, JM Zhao, JH Rao, R TI Interferometric measurements of variable 340 GHz linear polarization in Sagittarius A SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy : center; instrumentation : polarimeters; polarization; submillimeter; techniques : interferometric ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; SGR-A; CIRCULAR-POLARIZATION; SUBMILLIMETER EMISSION; INFRARED FLARES; RADIO-EMISSION; FLOW MODELS; ASTERISK AB Using the Submillimeter Array, we have made the first high angular resolution measurements of the linear polarization of Sagittarius A* at submillimeter wavelengths and the first detection of intraday variability in its linear polarization. We detected linear polarization at 340 GHz (880 mu m) at several epochs. At the typical resolution of 1".4; 2".2, the expected contamination from the surrounding (partially polarized) dust emission is negligible. We found that both the polarization fraction and the position angle are variable, with the polarization fraction dropping from 8.5% to 2.3% over 3 days. This is the first significant measurement of variability in the linear polarization fraction in this source. We also found variability in the polarization and total intensity within single nights, although the relationship between the two is not clear from these data. The simultaneous 332 and 342 GHz position angles are the same, setting a 1 sigma rotation measure (RM) upper limit of 7 x 10(5) rad m(-2). From position angle variations and comparison of "quiescent'' position angles observed here and at 230 GHz, we infer that the RM is a few times 10(5) rad m(-2), a factor of a few below our direct detection limit. A generalized model of the RM produced in the accretion flow suggests that the accretion rate at small radii must be low, below 10(-6)-10(-7) M-circle dot yr(-1) depending on the radial density and temperature profiles, but in all cases below the gas capture rate inferred from X-ray observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmarrone@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 NR 55 TC 92 Z9 93 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 MAR 20 PY 2006 VL 640 IS 1 BP 308 EP 318 DI 10.1086/500106 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100029 ER PT J AU Xu, YD Narayan, R Quataert, E Yuan, F Baganoff, FK AF Xu, YD Narayan, R Quataert, E Yuan, F Baganoff, FK TI Thermal X-ray iron line emission from the galactic center black hole Sagittarius A SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : nuclei; Galaxy : center radiation; mechanisms : thermal; X-rays : stars ID SGR-A; POINT SOURCES; ASTERISK; ACCRETION; CHANDRA; MODEL; FLOW; REGION; GALAXY; FLARE AB We model thermal X-ray emission from the accreting supermassive black hole Sagittarius A* at the Galactic center. For the region inside 1".5 of the center, we use a generalized radiatively inefficient accretion flow (RIAF) model, and for the region out to 1000 we use published models of the ambient hot gas. We calculate the equivalent widths of hydrogen-like and helium-like emission lines of various elements, notably iron. We predict that a strong helium-like iron line with an equivalent width similar to 1 keV should be emitted by both the external medium and the RIAF. The equivalent width in the external medium is sensitive to the metallicity Z of the gas as well as the mean temperature. For reasonable choices of these parameters, the calculated results agree with Chandra's detection of an iron line with an equivalent width of 1.3 keV within 10". The emission from within 1".5 is not sensitive to the external temperature, but is sensitive to the density and, especially, temperature profile inside the Bondi radius. For the range of profiles we consider, we calculate the equivalent width of the iron line to be similar to 0.6-1.5(Z/Z(circle dot)) keV, where Z(circle dot) is the solar metallicity. We present a new Chandra spectrum of the quiescent emission within 1".5 of Sgr A(*). The measured equivalent width of the iron line is 0.7 keV. Although this measurement has a large uncertainty, it is consistent with our predictions, provided the metallicity of the gas is approximately solar. C1 Shanghai Jiao Tong Univ, Dept Phys, Shanghai 200030, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Shanghai Jiao Tong Univ, Dept Phys, Shanghai 200030, Peoples R China. EM ydxu@sjtu.edu.cn; narayan@cfa.harvard.edu; eliot@astron.berkeley.edu; fyuan@physics.purdue.edu; fkb@space.mit.edu RI Xu, Yadi/O-1653-2015; OI Narayan, Ramesh/0000-0002-1919-2730 NR 34 TC 37 Z9 38 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 MAR 20 PY 2006 VL 640 IS 1 BP 319 EP 326 DI 10.1086/499932 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100030 ER PT J AU Seward, FD Williams, RM Chu, YH Dickel, JR Smith, RC Points, SD AF Seward, FD Williams, RM Chu, YH Dickel, JR Smith, RC Points, SD TI Chandra observation of the magellanic cloud supernova Remnant 0454-67.2 in N9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SNR 0454-67.2); supernova remnants; X-rays : ISM ID X-RAY PULSAR; RADIO-CONTINUUM; OB-ASSOCIATIONS; WIND NEBULA; EVOLUTION; DISCOVERY; KESTEVEN-79; ABUNDANCES; INTERIOR; EJECTA AB A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2.' 3 x 3.' 6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O III] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova ( SN) energy release was >= 5 x 10(50) ergs, and the age is similar to 3 x 10(4) yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Illinois, Urbana, IL 61801 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. RP Seward, FD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 11 Z9 11 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP 327 EP 334 DI 10.1086/499767 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100031 ER PT J AU Huard, TL Myers, PC Murphy, DC Crews, LJ Lada, CJ Bourke, TL Crapsi, A Evans, NJ McCarthy, DW Kulesa, C AF Huard, TL Myers, PC Murphy, DC Crews, LJ Lada, CJ Bourke, TL Crapsi, A Evans, NJ McCarthy, DW Kulesa, C TI Deep near-infrared observations of L1014: Revealing the nature of the core and its embedded source SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : globules; ISM : individual (L1014); reflection nebulae; stars : formation; stars : low-mass; brown dwarfs ID MILLIMETER-WAVE INTERFEROMETRY; AURIGA MOLECULAR CLOUD; YOUNG STELLAR CLUSTER; MASS STAR-FORMATION; SPACE-TELESCOPE; EVOLUTIONARY MODELS; INNER STRUCTURE; DENSE CORE; EXTINCTION; PROTOSTARS AB Recently, the Spitzer Space Telescope discovered L1014-IRS, a mid-infrared source with protostellar colors, toward the heretofore "starless'' core L1014. We present deep near-infrared observations that show a scattered light nebula extending from L1014-IRS. This nebula resembles those typically associated with protostars and young stellar objects, tracing envelope cavities presumably evacuated by an outflow. The northern lobe of the nebula has an opening angle of similar to 100 degrees, while the southern lobe is barely detected. Its morphology suggests that the bipolar cavity and inferred protostellar disk are not inclined more than 30 degrees from an edge-on orientation. The nebula extends at least 8" from the source at K-s, strongly suggesting that L1014-IRS is embedded within L1014 at a distance of 200 pc rather than in a more distant cloud associated with the Perseus arm at 2.6 kpc. In this case, the apparently low luminosity of L1014-IRS, 0.090 L-circle dot, is consistent with it having a substellar mass. However, if L1014-IRS is obscured by a circumstellar disk, its luminosity and inferred mass may be greater. Using near-infrared colors of background stars, we investigate characteristics of the L1014 molecular cloud core. We determine a mass of 3.6M(circle dot) for regions of the core with A(V) >= 2 mag. A comparison of the radial extinction profile of L1014 with other cores suggests that L1014 may be among the most centrally condensed cores known, perhaps indicative of the earliest stages of brown dwarf or star formation processes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Sci, Pasadena, CA 91101 USA. Univ Tennessee, Dept Geol Geog & Phys, Martin, TN 38238 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM thuard@cfa.harvard.edu; pmyers@cfa.harvard.edu; david@ociw.edu; lcrews@utm.edu; clada@cfa.harvard.edu; tbourke@cfa.harvard.edu; crapsi@arcetri.astro.it; nje@astro.as.utexas.edu; mccarthy@as.arizona.edu; ckulesa@as.arizona.edu NR 50 TC 41 Z9 41 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 MAR 20 PY 2006 VL 640 IS 1 BP 391 EP 401 DI 10.1086/498742 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100039 ER PT J AU Lorimer, DR Stairs, IH Freire, PC Cordes, JM Camilo, F Faulkner, AJ Lyne, AG Nice, DJ Ransom, SM Arzoumanian, Z Manchester, RN Champion, DJ van Leeuwen, J Mclaughlin, MA Ramachandran, R Hessels, JW Vlemmings, W Deshpande, AA Bhat, ND Chatterjee, S Han, JL Gaensler, BM Kasian, L Deneva, JS Reid, B Lazio, TJ Kaspi, VM Crawford, F Lommen, AN Backer, DC Kramer, M Stappers, BW Hobbs, GB Possenti, A D'Amico, N Burgay, M AF Lorimer, DR Stairs, IH Freire, PC Cordes, JM Camilo, F Faulkner, AJ Lyne, AG Nice, DJ Ransom, SM Arzoumanian, Z Manchester, RN Champion, DJ van Leeuwen, J Mclaughlin, MA Ramachandran, R Hessels, JW Vlemmings, W Deshpande, AA Bhat, ND Chatterjee, S Han, JL Gaensler, BM Kasian, L Deneva, JS Reid, B Lazio, TJ Kaspi, VM Crawford, F Lommen, AN Backer, DC Kramer, M Stappers, BW Hobbs, GB Possenti, A D'Amico, N Burgay, M TI Arecibo pulsar survey using ALFA. II. The young, highly relativistic binary pulsar J1906+0746 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; pulsars : individual (PSR J1906+0746) ID GEODETIC SPIN PRECESSION; DOUBLE NEUTRON-STARS; RADIO PULSARS; PROBABILITY-DISTRIBUTION; POSSIBLE COMPANIONS; COALESCENCE RATES; PSR J1141-6545; SYSTEM; DISCOVERY; B1913+16 AB We report the discovery of PSR J1906+0746, a young 144 ms pulsar in a highly relativistic 3.98 hr orbit with an eccentricity of 0.085 and expected gravitational wave coalescence time of similar to 300 Myr. The new pulsar was found during precursor survey observations with the Arecibo 1.4 GHz feed array system and retrospectively detected in the Parkes Multibeam plane pulsar survey data. From radio follow-up observations with Arecibo, Jodrell Bank, Green Bank, and Parkes, we have measured the spin-down and binary parameters of the pulsar and its basic spectral and polarization properties. We also present evidence for pulse profile evolution, which is likely due to geodetic precession, a relativistic effect caused by the misalignment of the pulsar spin and total angular momentum vectors. Our measurements show that PSR J1906+0746 is a young object with a characteristic age of 112 kyr. From the measured rate of orbital periastron advance (7 degrees 57 +/- 0 degrees.03 yr(-1)), we infer a total system mass of 2.61 +/- 0: 02 M-circle dot. While these parameters suggest that the PSR J1906+0746 binary system might be a younger version of the double pulsar system, intensive searches for radio pulses from the companion have so far been unsuccessful. It is therefore not known whether the companion is another neutron star or a massive white dwarf. Regardless of the nature of the companion, a simple calculation suggests that the Galactic birthrate of binaries similar to PSR J1906+ 0746 is similar to 60 Myr(-1). This implies that PSR J1906+0746 will make a significant contribution to the computed cosmic inspiral rate of compact binary systems. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Bryn Mawr Coll, Dept Phys, Rosemont, PA 19010 USA. Natl Radio Astron Observ, Charlottesville, VA USA. NASA, Goddard Space Flight Ctr, USRA, EUD, Greenbelt, MD 20771 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. USN, Res Lab, Washington, DC 20375 USA. Haverford Coll, Dept Phys, Haverford, PA 19041 USA. Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. Stichtung ASTRON, NL-7990 AA Dwingeloo, Netherlands. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Osservatorio Astron Cagliari, Ist Nazl Astrofis, I-09012 Capoterra, Italy. RP Lorimer, DR (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RI Gaensler, Bryan/F-8655-2010; D'Amico, Nichi/A-5715-2009; Deshpande, Avinash/D-4868-2012; Astronomy & Astrophysics Group, Raman Res Institute/D-4046-2012; Bhat, Ramesh/B-7396-2013 OI Burgay, Marta/0000-0002-8265-4344; Nice, David/0000-0002-6709-2566; Ransom, Scott/0000-0001-5799-9714; /0000-0002-2700-9916; Gaensler, Bryan/0000-0002-3382-9558; NR 50 TC 77 Z9 80 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP 428 EP 434 DI 10.1086/499918 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RE UT WOS:000236143100043 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ AF Brown, WR Geller, MJ Kenyon, SJ Kurtz, MJ TI A successful targeted search for hypervelocity stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; Galaxy : halo; Galaxy : kinematics and dynamics; Galaxy : stellar content; stars : early-type ID DIGITAL SKY SURVEY; MILKY-WAY HALO; GALACTIC-CENTER; BLACK-HOLE; MASS; EVOLUTION; VELOCITY; CLUSTER AB Hypervelocity stars (HVSs) travel with velocities so extreme that dynamical ejection from a massive black hole is their only suggested origin. Following the discovery of the first HVS by Brown and collaborators, we have undertaken a dedicated survey for more HVSs in the Galactic halo and present here the resulting discovery of two new HVSs: SDSS J091301.0 +/- 305120 and SDSS J091759.5 +/- 672238, traveling with Galactic rest-frame velocities of at least +558 +/- 12 and +638 +/- 12 km s(-1), respectively. Assuming the HVSs are B8 main-sequence stars, they are at distances of similar to 75 and similar to 55 kpc, respectively, and have travel times from the Galactic center consistent with their lifetimes. The existence of two B8 HVSs in our 1900 deg(2) survey, combined with the Yu & Tremaine HVS rate estimates, is consistent with HVSs drawn from a standard initial mass function but inconsistent with HVS drawn from a truncated mass function like the one in the top-heavy Arches cluster. The travel times of the five currently known HVSs provide no evidence for a burst of HVSs from a major infall event at the Galactic center in the last similar to 160 Myr. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu; mkurtz@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 33 TC 69 Z9 71 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP L35 EP L38 DI 10.1086/503279 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RG UT WOS:000236143300009 ER PT J AU Iono, D Peck, AB Pope, A Borys, C Scott, D Wilner, DJ Gurwell, M Ho, PTP Yun, MS Matsushita, S Petitpas, GR Dunlop, JS Elvis, M Blain, A Le Floc'h, E AF Iono, D Peck, AB Pope, A Borys, C Scott, D Wilner, DJ Gurwell, M Ho, PTP Yun, MS Matsushita, S Petitpas, GR Dunlop, JS Elvis, M Blain, A Le Floc'h, E TI Interferometric 890 mu m images of high-redshift submillimeter galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : formation; galaxies : high-redshift; galaxies : starburst; submillimeter ID HUBBLE-DEEP-FIELD; SCUBA SUPER-MAP; NUMBER COUNTS; LENSING CLUSTERS; SPACE-TELESCOPE; NORTH; CAMERA; STARBURSTS; EVOLUTION AB We present high-resolution 890 mu m images of two 20 mJy submillimeter galaxies, SMM J123711+622212 and MIPS J142824.0+352619, obtained using the Submillimeter Array (SMA). Using submillimeter interferometric observations with an angular resolution of 2".5, the coordinates of these high-redshift sources are determined with an accuracy of 0".2. The new SMA data on SMM J123711+622212 reveal an unresolved submillimeter source offset to the east by 0".8 from an optical galaxy found in deep HST images, suggesting either a large galaxy with a dusty central region or an interacting galaxy system. The SMA image of hyperluminous (L-FIR = 3.2 x 10(13) L-circle dot) source MIPS J142824.0+352619 provides a firm upper limit to the source size of less than or similar to 1".2. This constraint provides evidence that the foreground lens is only weakly affecting the observed high far-infrared luminosity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. CALTECH, Pasadena, CA 91125 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. Steward Observ, Tucson, AZ 85721 USA. RP Iono, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM d.iono@nao.ac.jp NR 35 TC 57 Z9 57 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP L1 EP L4 DI 10.1086/503290 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RG UT WOS:000236143300001 ER PT J AU Lada, CJ AF Lada, CJ TI Stellar multiplicity and the initial mass function: Most stars are single SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; stars : formation ID SOLAR-TYPE STARS; TRAPEZIUM CLUSTER; MAIN-SEQUENCE; BINARY STARS; M-DWARFS; LUMINOSITY FUNCTION; MOLECULAR CLOUDS; VISUAL BINARIES; SEARCH; EVOLUTION AB In this Letter I compare recent findings suggesting a low binary star fraction for late-type stars with knowledge concerning the forms of the stellar initial and present-day mass functions for masses down to the hydrogen-burning limit. This comparison indicates that most stellar systems formed in the Galaxy are likely single and not binary, as has been often asserted. Indeed, in the current epoch two-thirds of all main-sequence stellar systems in the Galactic disk are composed of single stars. Some implications of this realization for understanding the star and planet formation process are briefly mentioned. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu NR 46 TC 195 Z9 197 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP L63 EP L66 DI 10.1086/503158 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RG UT WOS:000236143300016 ER PT J AU Schnee, S Bethell, T Goodman, A AF Schnee, S Bethell, T Goodman, A TI Estimating the column density in molecular clouds with far-infrared and submillimeter emission maps SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : clouds; surveys ID INTERSTELLAR RADIATION-FIELD; DUST; TEMPERATURE; GRAINS AB We have used a numerical simulation of a turbulent cloud to synthesize maps of the thermal emission from dust at a variety of far-IR and submillimeter wavelengths. The average column density and external radiation field in the simulation is well matched to clouds such as Perseus and Ophiuchus. We use pairs of single-wavelength emission maps to derive the dust color temperature and column density, and we compare the derived column densities with the true column density. We demonstrate that longer wavelength emission maps yield less biased estimates of column density than maps made toward the peak of the dust emission spectrum. We compare the scatter in the derived column density with the observed scatter in Perseus and Ophiuchus. We find that while in Perseus all of the observed scatter in the emission-derived versus the extinction-derived column density can be attributed to the flawed assumption of isothermal dust along each line of sight, in Ophiuchus there is additional scatter above what can be explained by the isothermal assumption. Our results imply that variations in dust emission properties within a molecular cloud are not necessarily a major source of uncertainty in column density measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Schnee, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sschnee@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 13 TC 20 Z9 20 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2006 VL 640 IS 1 BP L47 EP L50 DI 10.1086/503292 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RG UT WOS:000236143300012 ER PT J AU Towe, KM AF Towe, KM TI Sea urchins as crystallographers SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Dept Paleobiol, Tennille, GA 31089 USA. RP Towe, KM (reprint author), Smithsonian Inst, Dept Paleobiol, 230 W Adams St, Tennille, GA 31089 USA. NR 4 TC 8 Z9 8 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 MAR 17 PY 2006 VL 311 IS 5767 BP 1554 EP 1555 DI 10.1126/science.311.5767.1554 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 022BK UT WOS:000236029500022 PM 16543442 ER PT J AU Isaza-Londono, C MacLeod, KG Huber, BT AF Isaza-Londono, C MacLeod, KG Huber, BT TI Maastrichtian North Atlantic warming, increasing stratification, and foraminiferal paleobiology at three timescales SO PALEOCEANOGRAPHY LA English DT Article ID CRETACEOUS PLANKTONIC-FORAMINIFERA; STABLE ISOTOPIC SIGNALS; BLAKE NOSE; OCEAN; PHOTOSYMBIOSIS; TRENDS; RECORD; EVENT; SIZE AB Analysis of 944 single specimens of three species of late Maastrichtian planktonic foraminifera (Racemiguembelina fructicosa, Contusotruncana contusa, and Rugoglobigerina rugosa) from 38 samples spanning the last 3 Myr of the Cretaceous shows consistent isotopic trends through time, consistent isotopic differences among taxa, and high within-sample isotopic variability throughout. Within-sample variability does not change systematically through time for any taxon, but average delta(18)O values decrease by similar to 1.5 parts per thousand, and average delta(13)C values diverge up section. Comparing taxa, average delta(18)O values are similar within most samples, but average delta(13)C values generally decrease from R. fructicosa to R. rugosa to C. contusa. In addition, the within-sample variability of individual delta(13)C measurements is larger for R. fructicosa than for either C. contusa or R. rugosa, an observation which is consistent with a photosymbiotic habitat for R. fructicosa. In terms of Maastrichtian paleoceanography the negative delta(18)O trend of similar to 1.5 parts per thousand corresponds to a temperature increase of similar to 6 degrees C, and the divergence of delta(13)C values up section suggests an increasingly stratified water column in the western Atlantic through the late Maastrichtian. We suggest that these trends are best explained by increasing import of South Atlantic waters into the North Atlantic and an intensification of the Northern Hemisphere polar front. C1 Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. Smithsonian Inst, Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Isaza-Londono, C (reprint author), Univ Missouri, Dept Geol Sci, 101 Geol Sci Bldg, Columbia, MO 65211 USA. EM ci3z4@mizzou.edu RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 NR 34 TC 14 Z9 14 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 J9 PALEOCEANOGRAPHY JI Paleoceanography PD MAR 15 PY 2006 VL 21 IS 1 AR PA1012 DI 10.1029/2004PA001130 PG 10 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA 026JM UT WOS:000236335200001 ER PT J AU Herre, EA AF Herre, EA TI Barcoding helps biodiversity fly SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID ARBUSCULAR MYCORRHIZAL FUNGI; HOST-SPECIFICITY; WASP MUTUALISM; DNA BARCODES; TAXONOMY; FOREST; DIVERSITY; TIME C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Apdo 0843-03092, Panama City, Panama. EM herrea@gamboa.si.edu NR 20 TC 9 Z9 9 U1 0 U2 2 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 14 PY 2006 VL 103 IS 11 BP 3949 EP 3950 DI 10.1073/pnas.0600550103 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 027QE UT WOS:000236429300002 PM 16537464 ER PT J AU Finlator, K Dave, R Papovich, C Hernquist, L AF Finlator, K Dave, R Papovich, C Hernquist, L TI The physical and photometric properties of high-redshift galaxies in cosmological hydrodynamic simulations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : evolution; galaxies : formation; galaxies : high-redshift; galaxies : photometry; galaxies : stellar content ID LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; ORIGINS DEEP SURVEY; ULTRAVIOLET LUMINOSITY DENSITY; EXTREMELY RED OBJECTS; DIGITAL SKY SURVEY; X-RAY-PROPERTIES; BLACK-HOLES; MIDINFRARED OBSERVATIONS; SUBSTANTIAL POPULATION AB We study the physical and photometric properties of galaxies at z = 4 in cosmological hydrodynamic simulations of a Lambda CDM universe. We focus on galaxies satisfying the `` B dropout'' criteria of the Great Observatories Origins DEEP Survey ( GOODS). Our simulations predict that high- redshift galaxies show strong correlations in star formation rate ( SFR) versus stellar mass, and weaker correlations versus environment and age, such that B dropouts are predicted to be the most massive, most rapidly star- forming galaxies at z 4, living preferentially in dense regions. The simulated rest- frame UV luminosity function ( LF) and integrated luminosity density are in broad agreement with observations at z similar to 4. The predicted faint- end slope is intrinsically steep but becomes shallower and is in reasonable agreement with data once GOODS selection criteria are imposed. At the bright end, there may be a modest excess of bright, rapidly star- forming galaxies. The predicted rest- frame optical LF is approximately 1 mag brighter than the rest- frame UV LF. We predict that GOODS B dropouts represent less than 50% of the total stellar mass density formed in galaxies more massive than log ( M (*) / M (circle dot)) > 87 by z = 4, mainly because of brightness limits in the HSTACS bands. Most of these results are somewhat sensitive to the effects of dust extinction. On average, simulated B dropouts are less metal enriched than observed low- redshift galaxies of similar stellar mass by approximate to 0.6 dex. Two simulated B dropouts exhibit SFRs exceeding 1000 M (circle dot) yr (- 1), similar to observed submillimeter galaxies. These galaxies are quite massive but are not undergoing starbursts; their SFRs only mildly exceed ( by similar to 2 - 3 times) the SFRs that would be expected for their stellar mass. Finally, the overall distribution of dust reddening and mean stellar age may be constrained from color- color plots although the specific value for each galaxy cannot. C1 Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Finlator, K (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM kfinlator@as.arizona.edu RI Finlator, Kristian/M-4809-2014 OI Finlator, Kristian/0000-0002-0496-1656 NR 95 TC 80 Z9 80 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP 672 EP 694 DI 10.1086/499349 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100008 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Robertson, B Di Matteo, T Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Robertson, B Di Matteo, T Springel, V TI The evolution in the faint-end slope of the quasar luminosity function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : active; galaxies : evolution; quasars : general ID ACTIVE GALACTIC NUCLEI; PARTICLE HYDRODYNAMICS SIMULATIONS; SUPERMASSIVE BLACK-HOLES; COSMOLOGICAL EVOLUTION; GALAXY FORMATION; PHYSICAL MODEL; HOST GALAXIES; ROSAT SURVEYS; MERGERS; AGN AB Using a new model for quasar lifetimes and light curves derived from numerical simulations of galaxy mergers that incorporate black hole growth, we study the faint- end slope of the quasar luminosity function ( QLF) and its evolution with redshift. Our model motivates a new interpretation of the QLF in which the bright end consists of quasars radiating near their peak luminosities but the faint end is mostly made up of brighter peak luminosity quasars seen in less luminous phases of evolution. The faint- end slope of the QLF is then set by the behavior of the lifetime ( light curve) of quasars with peak luminosities near the observed break when they are in less luminous stages of evolution. We determine the faint- end slope of the QLF from the quasar lifetime, based on a set of simulations that encompass a wide range of host galaxy, merger, black hole, and interstellar gas properties. Brighter peak luminosity ( higher black hole mass) systems undergo more violent evolution, and gas is expelled and heated more rapidly in the final stages of quasar evolution, resulting in a flatter faint- end slope ( as these objects fall below the observed break in the QLF more rapidly). Therefore, as the QLF break luminosity moves to higher luminosities with increasing redshift, implying a larger typical quasar peak luminosity, the faint- end QLF slope flattens. From our model, we predict the evolution of the faint- end slope of the QLF and find good agreement with observations. Although black holes grow in an antihierarchical manner ( with lower mass black holes formed primarily at lower redshifts), in our picture the observed change in slope and differential or `` luminosity- dependent density evolution'' in the QLF is determined by the nontrivial, luminosity- dependent quasar lifetime and physics of quasar feedback, and not by changes in the shape of the underlying peak luminosity or active black hole mass distributions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 67 TC 90 Z9 90 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP 700 EP 709 DI 10.1086/499351 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100010 ER PT J AU Kraft, RP Azcona, J Forman, WR Hardcastle, MJ Jones, C Murray, SS AF Kraft, RP Azcona, J Forman, WR Hardcastle, MJ Jones, C Murray, SS TI The hot gas environment of the radio galaxy 3C 388: Quenching the accumulation of cool gas in a cluster core by a nuclear outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (3C 388); galaxies : ISM; galaxies : jets; hydrodynamics; X-rays : galaxies : clusters ID X-RAY-EMISSION; MAGNETIC-FIELD STRENGTHS; INTRACLUSTER MEDIUM; THERMAL CONDUCTION; ELLIPTIC GALAXY; HYDRA-A; CHANDRA; FLOWS; LOBES; M87 AB We present results from a 35 ks Chandra ACIS-I observation of the hot intracluster medium (ICM) around the FR II radio galaxy 3C 388. 3C 388 resides in a cluster environment with an ICM temperature of similar to 3.5 keV. We detect cavities in the ICM coincident with the radio lobes. The enthalpy of these cavities is similar to 1.2 x 10(60) ergs. The work done on the gas by the inflation of the lobes is similar to 3 x 10(59) ergs, or similar to 0.87 keV per particle out to the radius of the lobes. The radiative timescale for gas at the center of the cluster at the current temperature is a few Gyr. The gas in the core was probably cooler and denser before the outburst, so the cooling time was considerably shorter. We are therefore likely to be witnessing the quenching of a cluster cooling flow by a radio galaxy outburst. The mechanical power of the lobes is at least 20 times larger than the radiative losses out to the cooling radius. Outbursts of similar power with a similar to 5% duty cycle would be more than sufficient to continually reheat the cluster core over the Hubble time and prevent the cooling of any significant amount of gas. The mechanical power of the outburst is also roughly 2 orders of magnitude larger than either the X-ray luminosity of the active nucleus or the radio luminosity of the lobes. The equipartition pressure of the radio lobes is more than an order of magnitude lower than that of the ambient medium, indicating that the pressure of the lobe is dominated by something other than the relativistic electrons radiating at GHz frequencies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, F-92195 Meudon, France. Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 NR 58 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 MAR 10 PY 2006 VL 639 IS 2 BP 753 EP 760 DI 10.1086/499488 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100016 ER PT J AU Li, YX Mac Low, MM Klessen, RS AF Li, YX Mac Low, MM Klessen, RS TI Star formation in isolated disk galaxies. II. Schmidt laws and efficiency of gravitational collapse SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : evolution; galaxies : ISM; galaxies : kinematics and dynamics; galaxies : spiral; galaxies : star clusters; stars : formation ID SMOOTHED PARTICLE HYDRODYNAMICS; TURBULENT MOLECULAR CLOUDS; COLD DARK-MATTER; ISOLATED BARRED GALAXIES; ANGULAR-MOMENTUM PROBLEM; FORMATION THRESHOLDS; SPIRAL GALAXIES; GALACTIC DISKS; INTERSTELLAR-MEDIUM; SECULAR EVOLUTION AB We model gravitational instability in a wide range of isolated disk galaxies, using GADGET, a three-dimensional, smoothed particle hydrodynamics code. The model galaxies include a dark matter halo and a disk of stars and isothermal gas. Absorbing sink particles are used to directly measure the mass of gravitationally collapsing gas. Below the density at which they are inserted, the collapsing gas is fully resolved. We make the assumption that stars and molecular gas form within the sink particle once it is created and that the star formation rate is the gravitational collapse rate times a constant efficiency factor. In our models, the derived star formation rate declines exponentially with time, and radial profiles of atomic and molecular gas and star formation rate reproduce observed behavior. We derive from our models and discuss both the global and local Schmidt laws for star formation: power-law relations between surface densities of gas and star formation rate. The global Schmidt law observed in disk galaxies is quantitatively reproduced by our models. We find that the surface density of star formation rate directly correlates with the strength of local gravitational instability. The local Schmidt laws of individual galaxies in our models show clear evidence of star formation thresholds. The variations in both the slope and the normalization of the local Schmidt laws cover the observed range. The averaged values agree well with the observed average and with the global law. Our results suggest that the nonlinear development of gravitational instability determines the local and global Schmidt laws and the star formation thresholds. We derive from our models the quantitative dependence of the global star formation efficiency on the initial gravitational instability of galaxies. The more unstable a galaxy is, the quicker and more efficiently its gas collapses gravitationally and forms stars. C1 Columbia Univ, Dept Astron, New York, NY 10027 USA. Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. Inst Astrophys, D-14482 Potsdam, Germany. RP Li, YX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yxli@cfa.harvard.edu; mordecai@amnh.org; rklessen@aip.de OI Mac Low, Mordecai-Mark/0000-0003-0064-4060 NR 121 TC 66 Z9 66 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP 879 EP 896 DI 10.1086/499350 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100027 ER PT J AU Chen, HR Welch, WJ Wilner, DJ Sutton, EC AF Chen, HR Welch, WJ Wilner, DJ Sutton, EC TI A high-mass protobinary system in the hot core W-3(H2O) SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : early-type; stars : individual (W-3(OH), W-3( H2O)); stars : pre-main-sequence ID EARLY-TYPE STARS; MOLECULAR CLOUDS; METHYL CYANIDE; CIRCUMSTELLAR DISKS; INTERSTELLAR-MEDIUM; DENSITY STRUCTURE; STELLAR OBJECTS; DUST CONTINUUM; YOUNG STARS; EMISSION AB We have observed a high- mass protobinary system in the hot core W3( H2O) with the BIMA array. Our continuum maps at wavelengths of 1.4 and 2.8 mm both achieve subarcsecond angular resolutions and show a double- peaked morphology. The angular separation of the two sources is 1".19, corresponding to 2: 43; 10(3) AU at the source distance of 2.04 kpc. The flux densities of the two sources at 1.4 and 2.8 mm have a spectral index of 3, translating to an opacity law of kappa(V) proportional to V. The small spectral indices suggest that grain growth has begun in the hot core. We have also observed five K components of the methyl cyanide ( CH3CN) J = 12 -> 11 transitions. A radial velocity difference of 2.81 +/- 0.10 km s (-1) is found toward the two continuum peaks. Interpreting these two sources as binary components in orbit about each other, we find a minimum mass of 22M(circle dot) for the system. Radiative transfer models are constructed to explain both the continuum and methyl cyanide line observations of each source. Power- law distributions of both density and temperature are derived. Density distributions close to the free- fall value, r (-1.5), are found for both components, suggesting continuing accretion. The derived luminosities suggest that the two sources have equivalent zero- age mainsequence ( ZAMS) spectral type B0.5 - B0. The nebular masses derived from the continuum observations are about 5 M (circle dot) for source A and 4 M-circle dot for source C. A velocity gradient previously detected may be explained by unresolved binary rotation with a small velocity difference. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Chen, HR (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23141, Taipei 106, Taiwan. EM hchen@asiaa.sinica.edu.tw; welch@astro.berkeley.edu; dwilner@cfa.harvard.edu; sutton@astro.uiuc.edu RI Sutton, Edmund/H-5113-2011 NR 61 TC 30 Z9 30 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP 975 EP 990 DI 10.1086/499395 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100035 ER PT J AU Silverstone, MD Meyer, MR Mamajek, EE Hines, DC Hillenbrand, LA Najita, J Pascucci, I Bouwman, J Kim, JS Carpenter, JM Stauffer, JR Backman, DE Moro-Martin, A Henning, T Wolf, S Brooke, TY Padgett, DL AF Silverstone, MD Meyer, MR Mamajek, EE Hines, DC Hillenbrand, LA Najita, J Pascucci, I Bouwman, J Kim, JS Carpenter, JM Stauffer, JR Backman, DE Moro-Martin, A Henning, T Wolf, S Brooke, TY Padgett, DL TI Formation and evolution of planetary systems (FEPS): Primordial warm dust evolution from 3 to 30 Myr around sun-like stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; planetary systems : protoplanetary disks; stars : formation; stars : pre-main-sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK MASSES; SCORPIUS OB ASSOCIATION; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; SOLAR-TYPE STARS; ALL-SKY SURVEY; X-RAY SOURCES AB We present data obtained with the Infrared Array Camera ( IRAC) aboard the Spitzer Space Telescope ( Spitzer) for a sample of 74 young (t < 30 Myr old) Sun- like (0: 7 < M-*/M circle dot < 1: 5) stars. These are a subset of the observations that comprise the Spitzer Legacy science program entitled the Formation and Evolution of Planetary Systems ( FEPS). Using IRAC, we study the fraction of young stars that exhibit 3.6 - 8.0 mu m infrared emission in excess of that expected from the stellar photosphere, as a function of age from 3 to 30 Myr. The most straightforward interpretation of such excess emission is the presence of hot ( 300 - 1000 K) dust in the inner regions (< 3 AU) of a circumstellar disk. Five out of the 74 young stars show a strong infrared excess, four of which have estimated ages of 3 - 10 Myr. While we detect excesses from five optically thick disks and photospheric emission from the remainder of our sample, we do not detect any excess emission from optically thin disks at these wavelengths. We compare our results with accretion disk fractions detected in previous studies and use the ensemble results to place additional constraints on the dissipation timescales for optically thick, primordial disks. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Max Planck Inst Astron, Heidelberg, Germany. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Princeton Univ, Princeton, NJ 08544 USA. RP Silverstone, MD (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 72 TC 75 Z9 75 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP 1138 EP 1146 DI 10.1086/499418 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LK UT WOS:000235837100049 ER PT J AU Huang, GL Lin, J AF Huang, GL Lin, J TI Quasi-periodic reversals of radio polarization at 17 GHz observed in the 2002 April 21 solar event SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization; Sun : activity; Sun : radio radiation ID CORONAL MASS EJECTION; NOBEYAMA RADIOHELIOGRAPH; MAGNETIC-FIELD; X1.5 FLARE; RHESSI; RECONNECTION; MICROWAVE; BURSTS; EMISSION; TRACE AB We investigate high spatial resolution radio polarization data obtained by the Nobeyama Radioheliograph (NoRH) and high time resolution data observed with the Nobeyama Radio Polarimeters (NoRP) during the well-studied flare/CME event of 2002 April 21. A 17 GHz radio source at the loop top was seen by NoRH to move upward together with the expanding flare loops at a speed of around 10 km s(-1). In the 5 minutes before the source began its upward motion, the Stokes V of the radio signals at 17 GHz showed quasi-periodic reversals between left-circular polarization (LCP) and right-circular polarization (RCP). Following this interval, the polarizations gradually turned to LCP. During this period, the polarization of the corresponding footpoint source maintained the RCP sense. The reversal of Stokes V between RCP and LCP was also detected at lower frequencies (1-2 GHz) by NoRP, without spatial resolution. The observed reversals between RCP and LCP of the radio signals from the top of the flare loop system can be taken as evidence that magnetic energy is released or energetic particles are produced at the magnetic reconnection site in a quasi-periodic fashion. C1 Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huang, GL (reprint author), Chinese Acad Sci, Purple Mt Observ, 2 W Beijing Rd, Nanjing 210008, Peoples R China. EM glhuang@pmo.ac.cn; jlin@cfa.harvard.edu RI LIN, JUN/B-9890-2017 NR 24 TC 14 Z9 15 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP L99 EP L102 DI 10.1086/502971 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LL UT WOS:000235837200014 ER PT J AU Lidz, A Oh, SP Furlanetto, SR AF Lidz, A Oh, SP Furlanetto, SR TI Have we detected patchy reionization in quasar spectra? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; intergalactic medium; large-scale structure of universe; quasars : absorption lines ID LY-ALPHA FOREST; GUNN-PETERSON TROUGH; COLD DARK-MATTER; INTERGALACTIC MEDIUM; APPROACHING REIONIZATION; SDSS J1148+5251; POWER-SPECTRUM; Z-SIMILAR-TO-6; CONSTRAINTS; EVOLUTION AB The Ly alpha forest at z greater than or similar to 5.5 shows strong scatter in the mean transmission even when smoothed over extremely large spatial scales, greater than or similar to 50 Mpc h(-1). This has been interpreted as a signature of strongly fluctuating radiation fields or patchy reionization. To test this claim, we calculate the scatter arising solely from density fluctuations, assuming a uniform ionizing background, via analytic arguments and simulations. This scatter alone is comparable to that observed. It rises steeply with redshift and is of order unity by, even on similar to 50 Mpc h(-1) scales. This arises z similar to 6 because (1) at, transmission spectra, which are sensitive mainly to rare voids, are highly biased ( with a linear z similar to 6 bias factor) tracers of underlying density fluctuations and (2) small-scale transverse modes are aliased to long- b >= 4 wavelength line-of-sight modes. Inferring patchy reionization from quasar spectra is therefore subtle and requires much more detailed modeling. Similarly, we expect density fluctuations alone to produce order unity transmission fluctuations in the He II Lya forest on the scales over which these measurements are typically made. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Lidz, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 46 Z9 46 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP L47 EP L50 DI 10.1086/502678 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LL UT WOS:000235837200001 ER PT J AU Reynolds, SP Borkowski, KJ Gaensler, BM Rea, N McLaughlin, M Possenti, A Israel, G Burgay, M Camilo, F Chatterjee, S Kramer, M Lyne, A Stairs, I AF Reynolds, SP Borkowski, KJ Gaensler, BM Rea, N McLaughlin, M Possenti, A Israel, G Burgay, M Camilo, F Chatterjee, S Kramer, M Lyne, A Stairs, I TI Discovery of the X-ray counterpart to the Rotating RAdio Transient J1819-1458 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (J1819-1458); radio continuum : stars; stars : flare; stars : neutron; X-rays : stars ID COHERENT TIMING SOLUTION; NEUTRON-STARS; PULSAR XTE-J1810-197; EMISSION; MAGNETAR; PROJECT; SURFACE; BURSTS; TORUS AB We present the discovery of the first X-ray counterpart to a Rotating RAdio Transient (RRAT) source. RRAT J1819-1458 is a relatively highly magnetized (G) member of a new class of unusual pulsar-like objects discovered by their bursting activity at radio wavelengths. A Chandra observation of that position revealed a pointlike source, CXOU J181934.1-145804, with a soft spectrum well fit by an absorbed blackbody with N-H = 7(-4)(+7) X 10(21)cm(-2), temperature kT = 0.12 +/- 0.04 keV, and an unabsorbed flux of similar to 2 X 10(-12) ergs cm(-2) s(-1) between 0.5 and 8 keV. No optical or infrared (IR) counterparts are visible within 1" of our X- ray position. The positional coincidence, spectral properties, and lack of an optical/IR counterpart make it highly likely that CXOU J181934.1 - 145804 is a neutron star and is the same object as RRAT J1819 - 1458. The source showed no variability on any timescale from the pulse period of 4.26 s up to the 5 day window covered by the observations, although our limits (especially for pulsations) are not particularly constraining. The X-ray properties of CXOU J181934.1 145804, while not yet measured to high precision, are similar to those of comparably aged radio pulsars and are consistent with thermal emission from a cooling neutron star. C1 N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. INAF, Osservatorio Astron Cagliari, I-09012 Capoterra, Italy. INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Reynolds, SP (reprint author), N Carolina State Univ, Dept Phys, POB 8202, Raleigh, NC 27695 USA. EM steve_reynolds@ncsu.edu; kborkow@unity.ncsu.edu; bgaensler@cfa.harvard.edu; n.rea@sron.nl; maura.mcLaughlin@manchester.ac.uk; possenti@ca.astro.it; gianluca@mporzio.astro.it; burgay@ca.astro.it; fernando@astro.columbia.edu; schatterjee@cfa.harvard.edu; mkramer@jb.man.ac.uk; agl@jb.man.ac.uk; stairs@physics.ubc.ca 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 NR 37 TC 49 Z9 49 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2006 VL 639 IS 2 BP L71 EP L74 DI 10.1086/502648 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LL UT WOS:000235837200007 ER PT J AU Laurance, WF AF Laurance, WF TI Diversity in tropical forests SO SCIENCE LA English DT Letter C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@si.edu RI Laurance, William/B-2709-2012 NR 0 TC 2 Z9 2 U1 1 U2 4 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 MAR 10 PY 2006 VL 311 IS 5766 BP 1376 EP 1376 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 022BJ UT WOS:000236029400014 PM 16527950 ER PT J AU Agnarsson, I Zhang, JX AF Agnarsson, I Zhang, JX TI New species of Anelosimus (Araneae : Theridiidae) from Africa and Southeast Asia, with notes on sociality and color polymorphism SO ZOOTAXA LA English DT Article DE cladistics; morphology; sociality; subsocial; taxonomy ID SUBSOCIAL SPIDER; NATAL DISPERSAL; EVOLUTION; PHYLOGENY; PATTERNS AB The cobweb spider genus Anelosimus contains species showing various levels of social behavior. American Anelosimus are well known and several species have been described from Europe, China, Japan, and Madagascar. However, to date, only two behaviorally unknown species have been described from continental Africa, Southeast Asia, and Australasia combined. In this paper we describe seven new Anelosimus species, A. agnar n. sp. (Malaysia), A. biglebowski n. sp. (Tanzania), A. dude n. sp. (Tanzania), A. linda n. sp. (Malaysia), A. monskenyensis n. sp. (Kenya), A. nelsoni n. sp. (South Africa), and A. sulawesi n. sp. (Sulawesi) from Africa and Southeast Asia. We also redescribe A. kohi Yoshida, 1993 and provide evidence for subsocial behavior in that species. Anelosimus kohi shows a marked color polymorphism that is apparently habitat-related, both in populations in Malaysia and in Singapore. Several of the undescribed species were included in previous phylogenetic analyses, and the likely phylogenetic placement of each species is discussed. Based on new behavioral information we discuss the phylogenetic and geographical distribution of temporary and permanent sociality in Anelosimus. C1 Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Washington, DC 20013 USA. RP Agnarsson, I (reprint author), Univ British Columbia, Dept Bot, 3529-6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM ingi@zoology.ubc.ca RI Zhang, Junxia/N-8409-2015 OI Zhang, Junxia/0000-0002-7937-1474 NR 28 TC 14 Z9 14 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 MAR 10 PY 2006 IS 1147 BP 1 EP 34 PG 34 WC Zoology SC Zoology GA 021IC UT WOS:000235975900001 ER PT J AU Smith, MA Woodley, NE Janzen, DH Hallwachs, W Hebert, PDN AF Smith, MA Woodley, NE Janzen, DH Hallwachs, W Hebert, PDN TI DNA barcodes reveal cryptic host-specificity within the presumed polyphagous members of a genus of parasitoid flies (Diptera : Tachinidae) SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Area de Conservacion Guanacaste; Belvosia; cytochrome c oxicase; internal transcribed spacer region 1; species richness ID BIOLOGICAL IDENTIFICATIONS; SEQUENCE ALIGNMENT; BIODIVERSITY; CONSERVATION; ECOLOGY AB Insect parasitoids are a major component of global biodiversity and affect the population dynamics of their hosts. However, identification of insect parasitoids is often difficult, and they are suspected to contain many cryptic species. Here, we ask whether the cytochrome c oxidase I DNA barcode could function as a tool for species identification and discovery for the 20 morphospecies of Belvosia parasitoid flies (Diptera: Tachinidae) that have been reared from caterpillars (Lepidoptera) in Area de Conservacion Guanacaste (ACG), northwestern Costa Rica. Barcoding not only discriminates among all 17 highly host-specific morphospecies of ACG Belvosia, but it also raises the species count to 32 by revealing that each of the three generalist species are actually arrays of highly host-specific cryptic species. We also identified likely hybridization among Belvosia by using a variable internal transcribed spacer region 1 nuclear rDNA sequence as a genetic covariate in addition to the strategy of overlaying barcode clusters with ecological information. If general, these results will increase estimates of global species richness and imply that tropical conservation and host-parasite interactions may be more complex than expected. C1 Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. Smithsonian Inst, USDA ARS, Washington, DC 20013 USA. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Smith, MA (reprint author), Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. EM salex@uoguelph.ca; djanzen@sas.upenn.edu RI Smith, M Alex/B-4468-2013; Hebert, Paul/C-4161-2013; Woodley, Norman/M-6160-2014 OI Smith, M Alex/0000-0002-8650-2575; Hebert, Paul/0000-0002-3081-6700; NR 29 TC 317 Z9 354 U1 7 U2 79 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 7 PY 2006 VL 103 IS 10 BP 3657 EP 3662 DI 10.1073/pnas.0511318103 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 024VU UT WOS:000236225300030 PM 16505365 ER PT J AU Archie, EA Moss, CJ Alberts, SC AF Archie, EA Moss, CJ Alberts, SC TI The ties that bind: genetic relatedness predicts the fission and fusion of social groups in wild African elephants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE social behaviour; population genetics; African elephant; kin selection; relatedness ID REPRODUCTIVE SUCCESS; ASSOCIATION; BEHAVIOR; SOCIOECOLOGY; ORGANIZATION; AMBOSELI; KINSHIP; SAMPLES; PCR AB Many social animals live in stable groups. In contrast, African savannah elephants (Loxodonta africana) live in unusually fluid, fission-fusion societies. That is, 'core' social groups are composed of predictable sets of individuals; however, over the course of hours or days, these groups may temporarily divide and reunite, or they may fuse with other social groups to form much larger social units. Here, we test the hypothesis that genetic relatedness predicts patterns of group fission and fusion among wild, female African elephants. Our study of a single Kenyan population spans 236 individuals in 45 core social groups, genotyped at 11 microsatellite and one mitochondrial DNA (mtDNA) locus. We found that genetic relatedness predicted group fission; adult females remained with their first order maternal relatives when core groups fissioned temporarily. Relatedness also predicted temporary fusion between social groups; core groups were more likely to fuse with each other when the oldest females in each group were genetic relatives. Groups that shared mtDNA haplotypes were also significantly more likely to fuse than groups that did not share mtDNA. Our results suggest that associations between core social groups persist for decades after the original maternal kin have died. We discuss these results in the context of kin selection and its possible role in the evolution of elephant sociality. C1 Duke Univ, Dept Geol, Durham, NC 27708 USA. Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Amboseli Elephant Res Project, Nairobi 00509, Kenya. RP Archie, EA (reprint author), Duke Univ, Dept Geol, POB 90338, Durham, NC 27708 USA. EM archiee@si.edu NR 46 TC 143 Z9 145 U1 13 U2 93 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2006 VL 273 IS 1586 BP 513 EP 522 DI 10.1098/rspb.2005.3361 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 010ZT UT WOS:000235238100001 PM 16537121 ER PT J AU Ishtiaq, F Beadell, JS Baker, AJ Rahmani, AR Jhala, YV Fleischer, RC AF Ishtiaq, F Beadell, JS Baker, AJ Rahmani, AR Jhala, YV Fleischer, RC TI Prevalence and evolutionary relationships of haematozoan parasites in native versus introduced populations of common myna Acridotheres tristis SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Acridotheres tristis; common myna; enemy release hypothesis; Haemoproteus; introduced; native ID BLOOD PARASITES; AVIAN MALARIA; HOST-SPECIFICITY; BIRDS; HEMATOZOA; PLASMODIUM; BIODIVERSITY; INFECTION; AVIFAUNA; ABSENCE AB The success of introduced species is frequently explained by their escape from natural enemies in the introduced region. We tested the enemy release hypothesis with respect to two well studied blood parasite genera (Plasmodium and Haemoproteus) in native and six introduced populations of the common myna Acridotheres tristis. Not all comparisons of introduced populations to the native population were consistent with expectations of the enemy release hypothesis. Native populations show greater overall parasite prevalence than introduced populations, but the lower prevalence in introduced populations is driven by low prevalence in two populations on oceanic islands (Fiji and Hawaii). When these are excluded, prevalence does not differ significantly. We found a similar number of parasite lineages in native populations compared to all introduced populations. Although there is some evidence that common mynas may have carried parasite lineages from native to introduced locations, and also that introduced populations may have become infected with novel parasite lineages, it may be difficult to differentiate between parasites that are native and introduced, because malarial parasite lineages often do not show regional or host specificity. C1 Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Royal Ontario Museum, Ctr Biodivers & Conservat Biol, Toronto, ON M5S 2C6, Canada. Bombay Natl Hist Soc, Bombay 400023, Maharashtra, India. Wildlife Inst India, Dehra Dun 248001, Uttar Pradesh, India. RP Ishtiaq, F (reprint author), Smithsonian Inst, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM ishtiaqf@si.edu FU NIGMS NIH HHS [1R01GM063258, R01 GM063258] NR 53 TC 38 Z9 38 U1 1 U2 26 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD MAR 7 PY 2006 VL 273 IS 1586 BP 587 EP 594 DI 10.1098/rspb.2005.3313 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 010ZT UT WOS:000235238100010 PM 16537130 ER PT J AU Murray, S Sanchez, CD Siemering, GH Enqvist, K Deem, SL AF Murray, S Sanchez, CD Siemering, GH Enqvist, K Deem, SL TI Transitional cell carcinoma of the urinary bladder in a spectacled bear (Tremarctos ornatus) SO VETERINARY RECORD LA English DT Article ID CANINE; PIROXICAM; CANCER; TRACT; MODEL; DOGS C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. SouthPaws Vet Referral Ctr, Springfield, VA 22150 USA. RP Murray, S (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001,Connecticut Ave NW, Washington, DC 20008 USA. NR 14 TC 0 Z9 1 U1 2 U2 5 PU BRITISH VETERINARY ASSOC PI LONDON PA 7 MANSFIELD ST, LONDON W1M 0AT, ENGLAND SN 0042-4900 J9 VET REC JI Vet. Rec. PD MAR 4 PY 2006 VL 158 IS 9 BP 306 EP 307 PG 2 WC Veterinary Sciences SC Veterinary Sciences GA 022RA UT WOS:000236072200013 PM 16517824 ER PT J AU Perry, L Sandweiss, DH Piperno, DR Rademaker, K Malpass, MA Umire, A de la Vera, P AF Perry, L Sandweiss, DH Piperno, DR Rademaker, K Malpass, MA Umire, A de la Vera, P TI Early maize agriculture and interzonal interaction in southern Peru SO NATURE LA English DT Article ID CAL KYR BP; AGE CALIBRATION; ORINOCO VALLEY; VENEZUELA; ECUADOR; REVEAL AB Over the past decade, increasing attention to the recovery and identification of plant microfossil remains from archaeological sites located in lowland South America has significantly increased knowledge of pre-Columbian plant domestication and crop plant dispersals in tropical forests and other regions(1-4). Along the Andean mountain chain, however, the chronology and trajectory of plant domestication are still poorly understood for both important indigenous staple crops such as the potato ( Solanum sp.) and others exogenous to the region, for example, maize (Zea mays)(5,6). Here we report the analyses of plant microremains from a late preceramic house (3,431 +/- 45 to 3,745 +/- 65 C-14 BP or similar to 3,600 to 4,000 calibrated years BP) in the highland southern Peruvian site of Waynuna. Our results extend the record of maize by at least a millennium in the southern Andes, show on-site processing of maize into flour, provide direct evidence for the deliberate movement of plant foods by humans from the tropical forest to the highlands, and confirm the potential of plant microfossil analysis in understanding ancient plant use and migration in this region. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA. Univ Maine, Dept Anthropol, Orono, ME 04469 USA. Univ Maine, Bryand Global Sci Ctr, Climate Change Inst, Orono, ME 04469 USA. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Ithaca Coll, Gannett Ctr G121, Dept Anthropol, Ithaca, NY 14850 USA. Museo Contisuyo, Moquegua, Peru. Inst Nacl Cultura, Arequipa, Peru. RP Perry, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, POB 37012,MRC 112, Washington, DC 20013 USA. EM perryli@si.edu NR 30 TC 65 Z9 71 U1 5 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 2 PY 2006 VL 440 IS 7080 BP 76 EP 79 DI 10.1038/nature04294 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 017HW UT WOS:000235685700042 PM 16511492 ER PT J AU Grissell, EE AF Grissell, E. E. TI A new species of Megastigmus Dalman (Hymenoptera : Torymidae), galling seed capsules of Eucalyptus camaldulensis Dehnhardt (Myrtaceae) in South Africa and Australia SO AFRICAN ENTOMOLOGY LA English DT Article DE Megastigmus; Eucalyptus; Syzygium; host adaptation; introduction ID NEW-ZEALAND; EULOPHIDAE AB The new species Megastigmus zebrinus Grissell is described based on specimens associated with seed capsules of Eucalyptus camaldulensis Dehnhardt (Myrtaceae), an endemic Australian tree. The wasp has been commonly collected in South Africa, where it was presumably introduced along with its host tree. It has apparently adapted to fruits of Syzygium cordatum Hochst. ex Krauss, an endemic South African tree in the same family as Eucalyptus. Observations on the gall-forming habit of Megastigmus zebrinus are presented based on dissections of Eucalyptus seed capsules. This appears to be the first species of Megastigmus that has been positively confirmed as a gall-former based on dissection of seed capsules. C1 Natl Museum Natl Hist, Smithsonian Inst, Systemat Entomol Lab, ARA USDA, Washington, DC 20013 USA. RP Grissell, EE (reprint author), Natl Museum Natl Hist, Smithsonian Inst, Systemat Entomol Lab, ARA USDA, CE 520,MRC168,POB 37012, Washington, DC 20013 USA. EM egrissel@sel.barc.usda.gov NR 22 TC 11 Z9 12 U1 0 U2 2 PU ENTOMOLOGICAL SOC SOUTHERN AFRICA PI HATFIELD PA PO BOX 13162, HATFIELD 0028, SOUTH AFRICA SN 1021-3589 J9 AFR ENTOMOL JI Afr. Entomol. PD MAR PY 2006 VL 14 IS 1 BP 87 EP 94 PG 8 WC Entomology SC Entomology GA 079KE UT WOS:000240174000009 ER PT J AU Keita, SOY Boyce, AJ AF Keita, SOY Boyce, AJ TI Variation in porotic hyperostosis in the Royal Cemetery complex at Abydos, Upper Egypt: a social interpretation SO ANTIQUITY LA English DT Article DE First Dynasty; Egypt; Abydos; cemetery; porotic hyperostosis ID DISEASE; AFRICA; ANEMIA; HEALTH AB Variation in the frequency and severity of porotic hyperostosis [porous defects], seen in the skulls of individuals buried at two First Dynasty cemeteries at Abydos, suggested differences in health and social conditions. Those buried near the kings had suffered from childhood deficiencies, while those associated with funerary enclosures in a second cemetery further to the north seemed to have benefited from occupational or social advantages. The author speculates on the possible factors which gave rise to this difference. C1 Howard Univ, Natl Human Genome Ctr, Washington, DC 20059 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Univ Oxford, Inst Biol Anthropol, Oxford OX1 2JD, England. Univ Oxford St Johns Coll, Oxford OX1 3JP, England. RP Keita, SOY (reprint author), Howard Univ, Natl Human Genome Ctr, Washington, DC 20059 USA. NR 36 TC 2 Z9 2 U1 0 U2 6 PU ANTIQUITY PI YORK PA KINGS MANOR, YORK YO1 7EP, ENGLAND SN 0003-598X J9 ANTIQUITY JI Antiquity PD MAR PY 2006 VL 80 IS 307 BP 64 EP 73 PG 10 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 023HR UT WOS:000236118100006 ER PT J AU Roubik, DW AF Roubik, David W. TI Stingless bee nesting biology SO APIDOLOGIE LA English DT Review DE meliponini; Apidae; nest architecture; nest microclimate; evolutionary ecology ID LOWLAND DIPTEROCARP FORESTS; SCAPTOTRIGONA-POSTICA; LESTRIMELITTA-LIMAO; APIDAE; HYMENOPTERA; MELIPONA; TRIGONA; GENUS; WAX; COLONY AB Stingless bees diverged since the Cretaceous, have 50 times more species than Apis, and are both distinctive and diverse. Nesting is capitulated by 30 variables but most do not define clades. Both architectural features and behavior decrease vulnerability, and large genera vary in nest habit, architecture and defense. Natural stingless bee colony density is 15 to 1500 km(-2). Symbionts include mycophagic mites, collembolans, leiodid beetles, mutualist coccids, molds, and ricinuleid arachnids. Mutualist bacteria and fungi preserve food and brood provisions. Nest associates include trees, termite, wasp and ant colonies. Ventilation is the means of nest environment regulation, achieved by fanning worker bees. Permanence of stingless bee nests, with annual mortality ca. 13%, implies a colony has 23 years to reproduce. Inability to freely swarm and single mating may all increase nesting specificity, competition, symbiosis and cleptobiosis in communities, while disease is rare. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Unit 0948, APO, AA 34002 USA. RP Roubik, DW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM roubikd@si.edu NR 113 TC 107 Z9 111 U1 3 U2 43 PU SPRINGER FRANCE PI PARIS PA 22 RUE DE PALESTRO, PARIS, 75002, FRANCE SN 0044-8435 EI 1297-9678 J9 APIDOLOGIE JI Apidologie PD MAR-APR PY 2006 VL 37 IS 2 BP 124 EP 143 DI 10.1051/apido:2006026 PG 20 WC Entomology SC Entomology GA 055UZ UT WOS:000238477400002 ER PT J AU Cortopassi-Laurino, M Imperatriz-Fonseca, VL Roubik, DW Dollin, A Heard, T Aguilar, I Venturieri, GC Eardley, C Nogueira-Neto, P AF Cortopassi-Laurino, Marilda Imperatriz-Fonseca, Vera Lucia Roubik, David Ward Dollin, Anne Heard, Tim Aguilar, Ingrid Venturieri, Giorgio C. Eardley, Connal Nogueira-Neto, Paulo TI Global meliponiculture: challenges and opportunities SO APIDOLOGIE LA English DT Review DE meliponiculture; stingless bees; breeding; honey; wax; pollinators; Apidae; Meliponini ID LOWLAND DIPTEROCARP FORESTS; STINGLESS BEES APIDAE; TROPICAL RAIN-FOREST; COSTA-RICA; MACADAMIA FLOWERS; APIS-MELLIFERA; MELIPONINI; POLLINATION; HONEY; HYMENOPTERA AB Stingless bees are social bees that live in tropical and subtropical areas of the world. All species produce honey, which has been appreciated by humans since ancient times. Here, the general panorama of meliponiculture is presented. Deforestation and poor management are the main problems faced by this incipient industry. For a profitable meliponiculture, much more biological information is needed, as well as field studies in natural conditions. In the near future, we suggest that the successful use of these pollinators will promote the development of new breeding techniques and commercialization possibilities, which must be designed to be sustainable. C1 Univ Sao Paulo, Inst Biosci, Dept Ecol, Sao Paulo, Brazil. Univ Sao Paulo, FFCL Ribeirao Preto, Dept Biol, BR-14040901 Ribeirao Preto, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Australian Nat Bee Res Ctr, N Richmond, NSW 2754, Australia. CSIRO Entomol, Indooroopilly, Qld 4068, Australia. Univ Nacl, CINAT, Heredia 4753000, Costa Rica. EMBRAPA Amazonia Oriental, BR-66017970 Belem, Para, Brazil. ARC Plant Protect Res Inst, ZA-0121 Queenswood, South Africa. RP Cortopassi-Laurino, M (reprint author), Univ Fed Santa Catarina, Ctr Biol Sci, BR-88040900 Florianopolis, SC, Brazil. EM mclaurin@usp.br RI Heard, Tim/B-1125-2008; Imperatriz-Fonseca, Vera/H-5582-2012 OI Heard, Tim/0000-0003-4975-7314; Imperatriz-Fonseca, Vera/0000-0002-1079-2158 NR 84 TC 50 Z9 52 U1 2 U2 22 PU SPRINGER FRANCE PI PARIS PA 22 RUE DE PALESTRO, PARIS, 75002, FRANCE SN 0044-8435 EI 1297-9678 J9 APIDOLOGIE JI Apidologie PD MAR-APR PY 2006 VL 37 IS 2 BP 275 EP 292 DI 10.1051/apido:2006027 PG 18 WC Entomology SC Entomology GA 055UZ UT WOS:000238477400011 ER PT J AU Nantais, JB Huchra, JP Barmby, P Olsen, KAG Jarrett, TH AF Nantais, JB Huchra, JP Barmby, P Olsen, KAG Jarrett, TH TI Nearby spiral globular cluster systems. I. Luminosity functions SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M31, NGC 55, NGC 247, NGC 253, NGC 300); galaxies : spiral; galaxies : star clusters; globular clusters : general ID HUBBLE-SPACE-TELESCOPE; RED GIANT BRANCH; MILKY-WAY; INFRARED PHOTOMETRY; ARAUCARIA-PROJECT; CEPHEID VARIABLES; GALAXIES; DISTANCES; INSIGHTS; SCULPTOR AB We compare the near-infrared (JHK) globular cluster luminosity functions (GCLFs) of the Milky Way, M31, and the Sculptor Group spiral galaxies. We obtained near-infrared photometry with the Persson's Auxiliary Nasmyth Infrared Camera on the Baade Telescope for 38 objects ( mostly globular cluster candidates) in the Sculptor Group. We also have near-infrared photometry from the Two Micron All Sky Survey (2MASS)-6X database for 360 M31 globular cluster candidates and aperture photometry for 96 Milky Way globular cluster candidates from the 2MASS All-Sky and Second Incremental Release databases. The M31 6X GCLFs peak at absolute reddening-corrected magnitudes of M(J0) = 9.18, M(H0) = -9.73, and M(K0) = -9.98. The mean brightness of the Milky Way objects is consistent with that of M31 after accounting for incompleteness. The average Sculptor absolute magnitudes ( correcting for relative distance from the literature and foreground reddening) are M(J0) = -9.18, M(H0) = -9.70, and M(K0) = -9.80. NGC 300 alone has absolute foreground-dereddened magnitudes M(J0) = -8.87, M(H0) = -9.39, and M(K0) = -9.46 using the newest Gieren et al. distance. This implies either that the NGC 300 GCLF may be intrinsically fainter than that of the larger galaxy M31 or that NGC 300 may be slightly farther away than previously thought. Straightforward application of our M31 GCLF results as a calibrator gives NGC 300 distance moduli of 26.68 +/- 0.14 using J, 26.71 +/- 0.14 using H, and 26.89 +/- 0.14 using K. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Nantais, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 50 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2006 VL 131 IS 3 BP 1416 EP 1425 DI 10.1086/500011 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RK UT WOS:000236143700017 ER PT J AU Lada, CJ Muench, AA Luhman, KL Allen, L Hartmann, L Megeath, T Myers, P Fazio, G Wood, K Muzerolle, J Rieke, G Siegler, N Young, E AF Lada, CJ Muench, AA Luhman, KL Allen, L Hartmann, L Megeath, T Myers, P Fazio, G Wood, K Muzerolle, J Rieke, G Siegler, N Young, E TI Spitzer observations of IC 348: The disk population at 2-3 million years SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; open clusters and associations : individual (IC 348) ID INFRARED ARRAY CAMERA; LOW-MASS STARS; T-TAURI STARS; SPECTRAL IRRADIANCE CALIBRATION; MULTIBAND IMAGING PHOTOMETER; YOUNG CLUSTER IC-348; SPACE-TELESCOPE; IC 348; ABSOLUTE CALIBRATION; ACCRETION DISKS AB We present near- and mid- infrared photometry obtained with the Spitzer Space Telescope of similar to 300 known members of the IC 348 cluster. We merge this photometry with existing ground- based optical and near- infrared photometry in order to construct optical- infrared spectral energy distributions ( SEDs) for all the cluster members and present a complete atlas of these SEDs. We employ these observations to investigate both the frequency and nature of the circumstellar disk population in the cluster. The Spitzer observations span a wavelength range between 3.6 and 24 mu m, corresponding to disk radii of similar to 0.1 - 5 AU from the central star. The observations are sufficiently sensitive to enable the first detailed measurement of the disk frequency for very low mass stars at the peak of the stellar initial mass function. Using measurements of infrared excess between 3.6 and 8.0 mu m, we find the total frequency of disk-bearing stars in the cluster to be 50% +/- 6%. However, only 30% +/- 4% of the member stars are surrounded by optically thick, primordial disks, while the remaining disk- bearing stars are surrounded by what appear to be optically thin, anemic disks. Both these values are below previous estimates for this cluster. The disk fraction appears to be a function of spectral type and stellar mass. The fraction of stars with optically thick disks ranges from 11% +/- 8% for stars earlier than K6 to 47% +/- 12% for K6 - M2 stars to 28% +/- 5% for M2 - M6 stars. The disk longevity and thus conditions for planet formation appear to be most favorable for the K6 - M2 stars, which are objects of comparable mass to the Sun for the age of this cluster. The optically thick disks around later type (> M4) stars appear to be less flared than the disks around earlier type stars. This may indicate a greater degree of dust settling and a more advanced evolutionary state for the late M disk population. Finally, we find that the presence of an optically thick dust disk is correlated with gaseous accretion, as measured by the strength of H alpha emission. A large fraction of stars classified as classical T Tauri stars possess robust, optically thick disks, and very few such stars are found to be diskless. The majority ( 64%) of stars classified as weak- lined T Tauri stars are found to be diskless. However, a significant fraction ( 12%) of these stars are found to be surrounded by thick, primordial disks. These results suggest that it is more likely for dust disks to persist in the absence of active gaseous accretion than for active accretion to persist in the absence of dusty disks. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Univ Arizona, Steward Observ, Tucson, AZ 85712 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu; gmuench@cfa.harvard.edu; kluhman@cfa.harvard.edu; lallen@cfa.harvard.edu; lhartmann@cfa.harvard.edu; tmegeath@cfa.harvard.edu; pmyers@cfa.harvard.edu; gfazio@cfa.harvard.edu; kw25@st-andrews.ac.uk; jamesm@as.arizona.edu; grieke@as.arizona.edu; eyoung@as.arizona.edu OI Muench, August/0000-0003-0666-6367 NR 45 TC 277 Z9 278 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2006 VL 131 IS 3 BP 1574 EP 1607 DI 10.1086/499808 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RK UT WOS:000236143700030 ER PT J AU Blondin, S Dessart, L Leibundgut, B Branch, D Hoflich, P Tonry, JL Matheson, T Foley, RJ Chornock, R Filippenko, AV Sollerman, J Spyromilio, J Kirshner, RP Wood-Vasey, WM Clocchiatti, A Aguilera, C Barris, B Becker, AC Challis, P Covarrubias, R Davis, TM Garnavich, P Hicken, M Jha, S Krisciunas, K Li, WD Miceli, A Miknaitis, G Pignata, G Prieto, JL Rest, A Riess, AG Salvo, ME Schmidt, BP Smith, RC Stubbs, CW Suntzeff, NB AF Blondin, S Dessart, L Leibundgut, B Branch, D Hoflich, P Tonry, JL Matheson, T Foley, RJ Chornock, R Filippenko, AV Sollerman, J Spyromilio, J Kirshner, RP Wood-Vasey, WM Clocchiatti, A Aguilera, C Barris, B Becker, AC Challis, P Covarrubias, R Davis, TM Garnavich, P Hicken, M Jha, S Krisciunas, K Li, WD Miceli, A Miknaitis, G Pignata, G Prieto, JL Rest, A Riess, AG Salvo, ME Schmidt, BP Smith, RC Stubbs, CW Suntzeff, NB TI Using line profiles to test the fraternity of Type Ia supernovae at high and low redshifts SO ASTRONOMICAL JOURNAL LA English DT Review DE cosmology : observations; line : formation; line : profiles; supernovae : general ID HUBBLE-SPACE-TELESCOPE; HIGH-VELOCITY EJECTA; OPTICAL-SPECTRA; LIGHT CURVES; SN 1994D; SPECTROSCOPIC OBSERVATIONS; INFRARED PHOTOMETRY; II SUPERNOVAE; TIME; CONSTRAINTS AB Using archival data of low- redshift ( z < 0. 01; Center for Astrophysics and SUSPECT databases) Type Ia supernovae ( SNe Ia) and recent observations of high- redshift ( 0. 16 < z < 0. 64) SNe Ia, we study the `` uniformity'' of the spectroscopic properties of nearby and distant SNe Ia. We find no difference in the measurements we describe here. In this paper we base our analysis solely on line- profile morphology, focusing on measurements of the velocity location of maximum absorption ( v(abs)) and peak emission ( v(peak)). Our measurement technique makes it easier to compare low and high signal- to- noise ratio observations. We also quantify the associated sources of error, assessing the effect of line blending with assistance from the parameterized code SYNOW. We find that the evolution of v(abs) and v(peak) for our sample lines ( Ca (II) lambda 3945, Si (II) k6355, and S (II) kk5454, 5640) is similar for both the low- and high- redshift samples. We find that vabs for the weak S (II) lambda lambda 5454, 5640 lines and v(peak) for S (II) lambda 5454 can be used to identify fast- declining [ Delta m(15)( B) > 1. 7] SNe Ia, which are also subluminous. In addition, we give the first direct evidence in two high- z SN Ia spectra of a double- absorption feature in Ca (II) lambda 3945, an event also observed, although infrequently, in low-redshift SN Ia spectra ( 6 out of 22 SNe Ia in our local sample). Moreover, echoing the recent studies of Dessart & Hillier in the context of Type II supernovae ( SNe II), we see similar P Cygni line profiles in our large sample of SN Ia spectra. First, the magnitude of the velocity location at maximum profile absorption may underestimate that at the continuum photosphere, as observed, for example, in the optically thinner line S (II) lambda 5640. Second, we report for the first time the unambiguous and systematic intrinsic blueshift of peak emission of optical P Cygni line profiles in SN Ia spectra, by as much as 8000 km s (-1). All the high- z SNe Ia analyzed in this paper were discovered and followed up by the ESSENCE collaboration and are now publicly available. C1 European So Observ, D-85748 Garching, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Texas, Dept Astron, Austin, TX 78681 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. AlbaNova, Stockholm Observ, SE-10691 Stockholm, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Univ Washington, Dept Phys, Seattle, WA 98195 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Blondin, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM sblondin@eso.org; luc@as.arizona.edu; bleibund@eso.org; branch@nhn.ou.edu; pah@hej1.as.utexas.edu; jt@ifa.hawaii.edu; matheson@noao.edu; rfoley@astro.berkeley.edu; chornock@astro.berkeley.edu; alex@astro.berkeley.edu; jesper@astro.su.se; jspyromi@eso.org; kirshner@cfa.harvard.edu; wmwood-vasey@cfa.harvard.edu; aclocchi@astro.puc.cl; caguilera@ctio.noao.edu; barris@ifa.hawaii.edu; becker@darkstar.astro.washington.edu; pchallis@cfa.harvard.edu; ricardo@astro.washington.edu; tamarad@mso.anu.edu.au; pgarnavi@nd.edu; mhicken@cfa.harvard.edu; sjha@astro.berkeley.edu; kkrisciu@nd.edu; weidong@astro.berkeley.edu; amiceli@astro.washington.edu; gm@u.washington.edu; prieto@astronomy.ohio-state.edu; arest@noao.edu; ariess@stsci.edu; salvo@mso.anu.edu.au; brian@mso.anu.edu.au; csmith@noao.edu; cstubbs@fas.harvard.edu; nsuntzeff@noao.edu RI Stubbs, Christopher/C-2829-2012; Davis, Tamara/A-4280-2008; OI Stubbs, Christopher/0000-0003-0347-1724; Davis, Tamara/0000-0002-4213-8783; Schmidt, Brian/0000-0001-6589-1287; Sollerman, Jesper/0000-0003-1546-6615; Schmidt, Brian/0000-0002-8538-9195 NR 105 TC 69 Z9 69 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2006 VL 131 IS 3 BP 1648 EP 1666 DI 10.1086/498724 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RK UT WOS:000236143700034 ER PT J AU Torres, G AF Torres, G TI The multiple system HD 27638 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; binaries : visual; stars : individual (HD 27638); stars : late-type; techniques : radial velocities; techniques : spectroscopic ID B-TYPE STARS; LINED SPECTROSCOPIC BINARIES; UVBY-BETA-PHOTOMETRY; T TAURI SECONDARIES; X-RAY-EMISSION; LOW-MASS STARS; EFFECTIVE TEMPERATURE; F-STARS; LITHIUM ABUNDANCES; RADIAL-VELOCITIES AB We report spectroscopic observations of HD 27638 B, the secondary in a visual binary in which the physically associated primary ( separation similar to 19") is a B9 V star. The secondary shows strong Li lambda 6708 absorption, suggesting youth, and has attracted attention in the past as a candidate post - T Tauri star, although this has subsequently been ruled out. It was previously known to be a double- lined spectroscopic binary ( F8+ G6) with a period of 17.6 days and to show velocity residuals indicating a more distant massive third companion with a period of at least 8 yr. Based on our radial velocity measurements covering more than two cycles of the outer orbit, along with other measurements, we derive an accurate triple orbital solution giving an outer period of 9. 447 +/- 0. 017 yr. The third object is more massive than either of the other two components of HD 27638 B but is not apparent in the spectra. We derive absolute visual magnitudes and effective temperatures for the three visible stars in HD 27638. Isochrone fitting based on those properties gives an age of 200 +/- 50 Myr for the system. We also infer an inclination angle of similar to 53 degrees 3 for the inner orbit of HD 27638 B. We detect a near- infrared excess in HD 27638 B, which we attribute to the third star being a close binary composed of late- type stars. This explains its large mass and lack of a visible signature. Modeling of this excess allows us to infer not only the masses of the components of the unseen companion but also the inclination angle of the outer orbit ( similar to 73 degrees). The HD 27638 system is thus at least quintuple. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 51 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2006 VL 131 IS 3 BP 1702 EP 1711 DI 10.1086/500355 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RK UT WOS:000236143700039 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Terrestrial planet formation. I. The transition from oligarchic growth to chaotic growth SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID ISOTHERMAL GASEOUS DISK; KUIPER-BELT OBJECTS; SOLAR NEBULA; GAS DISK; 3-DIMENSIONAL INTERACTION; GRAVITATIONAL SCATTERING; ACCRETIONAL EVOLUTION; RUNAWAY GROWTH; PLANETESIMALS; PROTOPLANETS AB We use a hybrid, multiannulus, n-body-coagulation code to investigate the growth of kilometer-sized planetesimals at 0.4-2 AU around a solar-type star. After a short runaway growth phase, protoplanets with masses of similar to 10(26) g and larger form throughout the grid. When (1) the mass in these "oligarchs'' is roughly comparable to the mass in planetesimals and (2) the surface density in oligarchs exceeds 2-3 g cm(-2) at 1 AU, strong dynamical interactions among oligarchs produce a high merger rate, which leads to the formation of several terrestrial planets. In disks with lower surface density, milder interactions produce several lower-mass planets. In all disks, the planet formation timescale is similar to 10-100 Myr, similar to estimates derived from the cratering record and radiometric data. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X NR 68 TC 116 Z9 116 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2006 VL 131 IS 3 BP 1837 EP 1850 DI 10.1086/499807 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 023RK UT WOS:000236143700052 ER PT J AU Rodriguez-Martinez, M Velazquez, PF Binette, L Raga, AC AF Rodriguez-Martinez, M Velazquez, PF Binette, L Raga, AC TI Precessing jets from a moving source and bright X-ray filaments in galaxy clusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE hydrodynamics; methods : numerical; galaxies : jets; X-rays : galaxies : clusters ID COOLING FLOW CLUSTERS; EXTRAGALACTIC JETS; ABELL 1795; MAGNETOHYDRODYNAMIC MODELS; SUPERNOVA-REMNANTS; ATOMIC DATABASE; EMISSION-LINES; RADIO; ELEMENTS; OUTFLOW AB We present hydrodynamical calculations carried out with the 3D YGUAZU-A code for a precessing jet model that is interacting with a plane parallel wind. This scenario describes an extragalactic jet in which the jet source is in motion with respect to the surrounding intra-cluster medium. From the numerical results, synthetic emission maps and spectra in X-ray band were obtained. We compare these predictions with observations of the radio jets emanating from the radio-galaxy 4C 26.42 ( in the Abell 1795 galaxy cluster). We find that the general morphology of the radio jets can be described by a point-symmetric precessing jet system interacting with a plane parallel wind (i.e., the intra-cluster medium flowing past the galaxy). We also find that our synthetic X-ray emission maps reproduce the observed large scale structures ( with sizes on the order of tens of kpc). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Rodriguez-Martinez, M (reprint author), Harvard Smithsonian Ctr Astrophys, MS-83,60 Garden St, Cambridge, MA 02138 USA. EM mario@head.cfa.harvard.edu; pablo@nucleares.unam.mx; binette@astroscu.unam.mx; raga@nucleares.unam.mx OI Rodriguez-Martinez, Mario/0000-0002-5358-0681 NR 33 TC 7 Z9 7 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 MAR PY 2006 VL 448 IS 1 BP 15 EP 21 DI 10.1051/0004-6361:20053382 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018PP UT WOS:000235777600003 ER PT J AU Lebron, M Beuther, H Schilke, P Stanke, T AF Lebron, M Beuther, H Schilke, P Stanke, T TI The extremely high-velocity molecular outflow in IRAS 20126+4104 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; ISM : jets and outflows; ISM : individual objects : IRAS 20126+4104 ID CO LINE FORMATION; IRAS 20126+4104; BIPOLAR FLOWS; SYSTEM; JET; REGIONS; GAS AB New sensitive CO(2 - 1) observations of the massive star-forming region IRAS 20126+ 4104 reveal a high-velocity gas component that has not been observed before. Comparing the morphologies of the high-velocity CO and the molecular jet traced by H-2 and SiO, we found various orientations projected on the plane of the sky that could be interpreted in terms of jet precession. The outflow shows a steepening mass spectrum with increasing flow velocities. The high-velocity gas in IRAS 20126+ 4104 contributes significantly to the energy and momentum of the flow. C1 Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Lebron, M (reprint author), Natl Astron & Ionosphere Ctr, Arecibo Observ, HC 03 Box 53995, Arecibo, PR 00612 USA. EM mlebron@naic.edu NR 25 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 MAR PY 2006 VL 448 IS 3 BP 1037 EP 1042 DI 10.1051/0004-6361:20041852 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018PR UT WOS:000235777800023 ER PT J AU Bensch, F AF Bensch, F TI Neutral carbon and CO emission in the core and the halo of dark cloud Barnard 5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : abundances; astrochemistry; ISM : clouds; ISM : individual : B5; radio lines : ISM ID INTERSTELLAR MOLECULAR-HYDROGEN; SMALL-SCALE STRUCTURE; STAR-FORMING REGIONS; IRAM KEY-PROJECT; BEAM PICK-UP; ROTATIONAL-EXCITATION; ATOMIC CARBON; H-I; MAPPING OBSERVATIONS; LINE EMISSION AB Aims. The physical conditions and chemical structure in the dark cloud of Barnard 5 and its surrounding atomic halo is studied. The impact of the halo on the line emission emerging from the molecular cloud is investigated. Methods. We present observations of the [CI] P-3(1) --> P-3(0) transition of neutral carbon and the low-J transitions of (CO)-C-12 and (CO)-C-13. The CO maps extend from the core (A(v) greater than or similar to 7) to the northern cloud edge and into the halo (A(v) less than or similar to 1). They are complemented by deeply integrated [CI] spectra made along a 1D cut of similar extent. Escape probability and photon-dominated region (PDR) models are employed to interpret the observations. Results. (CO)-C-12 and (CO)-C-13 are detected in the cloud and the halo, while [ CI] is detected only toward the molecular cloud. This occurs even though the neutral carbon column density is greater than or similar to 5 times larger than the CO column density in the halo, but it can be understood in terms of excitation. The [ CI] excitation is governed by collisions even at the low halo densities, while the CO excitation is dominated by the absorption of line photons emitted by the nearby molecular cloud. The upper limit on the neutral carbon column density in the halo is 6 x 10(15) cm(-2). The PDR studies show that even small column densities of H-2 and CO, such as those in the B5 halo, can significantly change the [CI] and CO line emission (pre-shielding). Since this effect decreases the [CI] intensity and increases the CO intensity, the largest impact is noted for the [CI]/CO line ratios. For the B5 cloud, a PDR model with a molecular hydrogen column density of similar to 6 x 10(19) cm(-2) in the halo matches the observed [CI]/CO line ratios best. Models with no pre-shielding, in contrast, suggest high gas densities that are in conflict with independently derived densities. The PDR models with a(chi) < 1 demonstrate that the [CI]/ CO ratios cannot be attributed solely to a reduced FUV field. C1 Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. RP Bensch, F (reprint author), Univ Bonn, Inst Radioastron, Hugel 71, D-53121 Bonn, Germany. EM fbensch@astro.uni-bonn.de NR 58 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 MAR PY 2006 VL 448 IS 3 BP 1043 EP 1060 DI 10.1051/0004-6361:20053580 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018PR UT WOS:000235777800024 ER PT J AU in't Zand, JJM Jonker, PG Nelemans, G Steeghs, D O'Brien, K AF in't Zand, JJM Jonker, PG Nelemans, G Steeghs, D O'Brien, K TI Optical identification of IGR J19140+0951 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : binaries; X-rays : individuals : EXO 1912+098, IGR J19140+0951, 2MASS 19140422+0952577 ID X-RAY BINARIES; IGR-J19140+0951; CATALOG AB IGR J19140+0951 was discovered by INTEGRAL in 2003 in the 4-100 keV band. Observations with INTEGRAL and RXTE provide a tentative identification as a high-mass X-ray binary (HMXB) with a neutron star as accretor. However, an optical counterpart was thus far not established, nor was the presence of a pulsar which is commonly observed in HMXBs. We observed IGR J19140+0951 with Chandra and find the source to be active at a similar flux as previous measurements. The lightcurve shows a marginally significant oscillation at 6.5 ks which requires confirmation. We determine a sub-arcsecond position from the Chandra data and identify the heavily reddened optical counterpart 2MASS 19140422+0952577 in the 2MASS catalog. Optical follow-up observations with the William Herschel Telescope at La Palma exhibit a continuum spectrum coming out of extinction above 7000 angstrom without strong absorption or emission features. V, I and K(s) band photometry point to an optical counterpart with an extinction of A(V) = 11 +/- 2. The extinction is consistent with the interstellar value. None of the data reject the suspicion that IGR J19140+0951 is an HMXB with additional circumstellar obscuration around the accretor. C1 SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02198 USA. Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. European So Observ, Santiago, Chile. RP in't Zand, JJM (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM jeanz@sron.nl RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746 NR 25 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 MAR PY 2006 VL 448 IS 3 BP 1101 EP 1106 DI 10.1051/0004-6361:20053411 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018PR UT WOS:000235777800029 ER PT J AU Mueller, M Harris, AW Bus, SJ Hora, JL Kassis, M Adams, JD AF Mueller, M Harris, AW Bus, SJ Hora, JL Kassis, M Adams, JD TI The size and albedo of Rosetta fly-by target 21 Lutetia from new IRTF measurements and thermal modeling SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids; infrared : solar system; radiation mechanisms : thermal ID SPECTRAL IRRADIANCE CALIBRATION; ASTEROIDS; 21-LUTETIA; STANDARDS; MISSION; NETWORK; PHYSICS AB Recent spectroscopic observations indicate that the M-type asteroid 21 Lutetia has a primitive, carbonaceous-chondrite-like (C-type) surface composition for which a low geometric albedo would be expected; this is incompatible with the IRAS albedo of 0.221 +/- 0.020. From new thermal-infrared spectrophotometric measurements and detailed thermophysical modeling we infer that Lutetia has a diameter of 98.3 +/- 5.9 km and a geometric albedo of 0.208 +/- 0.025, in excellent agreement with the IRAS value. We can thus rule out a low albedo typical of a C-type taxonomic classification. Furthermore, we find that Lutetia's thermal properties are well within the range expected for large asteroids; we find no evidence for unusually high thermal inertia. C1 DLR, Inst Planetary Res, D-12489 Berlin, Germany. Inst Astron, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Keck Observ, Kamuela, HI 96743 USA. Cornell Univ, Ithaca, NY 14853 USA. RP Mueller, M (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM michael.mueller@dlr.de OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650 NR 29 TC 38 Z9 38 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 MAR PY 2006 VL 447 IS 3 BP 1153 EP 1158 DI 10.1051/0004-6361:20053742 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018PO UT WOS:000235777500030 ER PT J AU Kessler-Silacci, J Augereau, JC Dullemond, CP Geers, V Lahuis, F Evans, NJ van Dishoeck, EF Blake, GA Boogert, ACA Brown, J Jorgensen, JK Knez, C Pontoppidan, KM AF Kessler-Silacci, J Augereau, JC Dullemond, CP Geers, V Lahuis, F Evans, NJ van Dishoeck, EF Blake, GA Boogert, ACA Brown, J Jorgensen, JK Knez, C Pontoppidan, KM TI c2d Spitzer IRS spectra of disks around T Tauri stars. I. Silicate emission and grain growth SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : ISM; ISM : lines and bands; solar system : formation; stars : formation; stars : pre-main-sequence ID MAIN-SEQUENCE STARS; HERBIG AE/BE STARS; H-ALPHA EMISSION; YOUNG STELLAR OBJECTS; ISO SPECTROSCOPY; MOLECULAR CLOUDS; ACCRETION DISKS; CHAMELEON-I; CRYSTALLINE SILICATES; ENERGY-DISTRIBUTIONS AB Infrared similar to 5-35 mu m spectra for 40 solar mass T Tauri stars and 7 intermediate-mass Herbig Ae stars with circumstellar disks were obtained using the Spitzer Space Telescope as part of the c2d IRS survey. This work complements prior spectroscopic studies of silicate infrared emission from disks, which were focused on intermediate-mass stars, with observations of solar mass stars limited primarily to the 10 mu m region. The observed 10 and 20 mu m silicate feature strengths/shapes are consistent with source-to-source variations in grain size. A large fraction of the features are weak and flat, consistent with micron-sized grains indicating fast grain growth (from 0.1 to 1.0 mu m in radius). In addition, approximately half of the T Tauri star spectra show crystalline silicate features near 28 and 33 mu m, indicating significant processing when compared to interstellar grains. A few sources show large 10-to-20 mu m ratios and require even larger grains emitting at 20 mu m than at 10 mu m. This size difference may arise from the difference in the depth into the disk probed by the two silicate emission bands in disks where dust settling has occurred. The 10 mu m feature strength versus shape trend is not correlated with age or H alpha equivalent width, suggesting that some amount of turbulent mixing and regeneration of small grains is occurring. The strength versus shape trend is related to spectral type, however, with M stars showing significantly flatter 10 mu m features (larger grain sizes) than A/B stars. The connection between spectral type and grain size is interpreted in terms of the variation in the silicate emission radius as a function of stellar luminosity, but could also be indicative of other spectral-type-dependent factors (e.g., X-rays, UV radiation, and stellar/disk winds). C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. Max Planck Inst Astrophys, D-85741 Garching, Germany. SRON, NL-9700 AV Groningen, Netherlands. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Prod Engn, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM jes@astro.as.utexas.edu OI Dullemond, Cornelis/0000-0002-7078-5910 NR 86 TC 176 Z9 176 U1 0 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 MAR 1 PY 2006 VL 639 IS 1 BP 275 EP 291 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LI UT WOS:000235836900022 ER PT J AU Lee, CF Ho, PTP Beuther, H Bourke, TL Zhang, QZ Hirano, N Shang, H AF Lee, CF Ho, PTP Beuther, H Bourke, TL Zhang, QZ Hirano, N Shang, H TI Infall and outflow around the HH 212 protostellar system SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (HH 212); ISM : jets and outflows; stars : formation ID YOUNG STELLAR OBJECTS; STAR-FORMATION; JET-DRIVEN; HL TAURI; ENVELOPE; COLLAPSE; DISK; GAS; CANDIDATES; ROTATION AB HH212 is a highly collimated jet discovered in H-2 powered by a young Class 0 source, IRAS 05413-0104, in the L1630 cloud of Orion. We have mapped around it in 1.33 mm continuum, (CO)-C-12 (J = 2-1), (CO)-C-13 (J = 2-1), (CO)-O-18 (J = 2-1), and SO (N-J = 5(6)-4(5)) emission at similar to 2."5 resolution with the Submillimeter Array. A dust core is seen in the continuum around the source. A flattened envelope is seen in (CO)-O-18 around the source in the equator perpendicular to the jet axis, with its inner part seen in (CO)-C-13. The structure and kinematics of the envelope can be roughly reproduced by a simple edge-on disk model with both infall and rotation. In this model, the density of the disk is assumed to have a power-law index of p = -1.5 or -2, as found in other low-mass envelopes. The envelope seems dynamically infalling toward the source with slow rotation because the kinematics is found to be roughly consistent with a free fall toward the source plus a rotation of a constant specific angular momentum. A (CO)-C-12 outflow is seen surrounding the H-2 jet, with a narrow waist around the source. Jetlike structures are also seen in (CO)-C-12 near the source aligned with the H-2 jet at high velocities. The morphological relationship between the H-2 jet and the (CO)-C-12 outflow, and the kinematics of the (CO)-C-12 outflow along the jet axis, are both consistent with those seen in a jet-driven bow shock model. SO emission is seen around the source and the H-2 knotty shocks in the south, tracing shocked emission around them. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Harvard Smithsonian Ctr Astrophys, Submillimeter Array,645 N Aohoku Pl, Hilo, HI 96720 USA. EM cflee@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 32 TC 41 Z9 41 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 MAR 1 PY 2006 VL 639 IS 1 BP 292 EP 302 DI 10.1086/499297 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LI UT WOS:000235836900023 ER PT J AU Fontenla, JM Avrett, E Thuillier, G Harder, J AF Fontenla, JM Avrett, E Thuillier, G Harder, J TI Semiempirical models of the solar atmosphere. I. The quiet- and active sun photosphere at moderate resolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : atmosphere ID TRANSITION REGION; ENERGY-BALANCE; SPECTRAL IRRADIANCE; SOLSPEC SPECTROMETER; STELLAR ATMOSPHERES; ULTRAVIOLET OPACITY; MAGNETIC REGIONS; SUNSPOT PENUMBRA; OH LINES; CHROMOSPHERE AB In this paper we study and modify previous semiempirical models of the solar photosphere as observed at moderate spatial and temporal resolution (similar to 3" and similar to 30 minutes, respectively) in the main quiet- and active Sun component features. Our present models are constructed to match the relevant available observations at this resolution for which a one-dimensional and time-independent stratification is reasonable. The models do not describe the fine structure and temporal variability observed in high-resolution images but correspond to a "radiation averaging'' over the fine-structure and p-mode variations. We use the observed limb darkening in the range 0.3-2.4 mu m, as well as the absolute intensities and details of the spectral continua and lines in this range, to validate and adjust the models. Using the method described in a previous paper, we compute the emergent radiation from our models in full detail for the visible and IR continuum and the lines in the interval 0.3-5 mu m for which we have atomic data from NIST (similar to 13,000 lines used) and molecular data from HITRAN and Gray & Corbally (similar to 480,000 molecular lines used). The observations, abundances, and atomic/molecular data are improved over previous work and yield models that better fit the observations. In addition, we construct a new penumbra model. The visible and IR detailed spectra computed from these models provide insight for understanding the effects of magnetic fields on the solar irradiance and are useful tools for computing synthetic spectral irradiances in different solar activity configurations. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. RP Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. EM fontenla@lasp.colorado.edu NR 68 TC 95 Z9 95 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2006 VL 639 IS 1 BP 441 EP 458 DI 10.1086/499345 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LI UT WOS:000235836900040 ER PT J AU Brogan, CL Gelfand, JD Gaensler, BM Kassim, NE Lazio, TJW AF Brogan, CL Gelfand, JD Gaensler, BM Kassim, NE Lazio, TJW TI Discovery of 35 new supernova remnants in the inner galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum : ISM; supernova remnants; surveys ID GALACTIC PLANE SURVEY; EMISSION; CATALOG AB We report the discovery of up to 35 new supernova remnants (SNRs) from a 42'' resolution, 90 cm multiconfiguration Very Large Array survey of the Galactic plane covering 4.degrees 5 < l < 22.degrees 0 and vertical bar b vertical bar < 1.degrees 25. Archival 20 cm, 11 cm, and 8 mm data have also been used to identify the SNRs and constrain their properties. The 90 cm image is sensitive to SNRs with diameters 2.'5 to 50' and down to a surface brightness limit of similar to 10(-21) W m(-2) Hz(-1) sr(-1). This survey has nearly tripled the number of SNRs known in this part of the Galaxy and represents an overall 15% increase in the total number of Galactic SNRs. These results suggest that further deep, low-frequency surveys of the inner Galaxy will resolve the discrepancy between the expected number of Galactic SNRs and the significantly smaller number of currently known SNRs. C1 Inst Astron, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. RP Brogan, CL (reprint author), Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. EM cbrogan@ifa.hawaii.edu RI Gaensler, Bryan/F-8655-2010; Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Gaensler, Bryan/0000-0002-3382-9558 NR 25 TC 86 Z9 86 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2006 VL 639 IS 1 BP L25 EP L29 DI 10.1086/501500 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 019LJ UT WOS:000235837000007 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Di Matteo, T Robertson, B Springel, V TI A unified, merger-driven model of the origin of starbursts, quasars, the cosmic X-ray background, supermassive black holes, and galaxy spheroids SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei; quasars : general ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; LY-ALPHA FOREST; ULTRALUMINOUS INFRARED GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; NEARBY LUMINOUS QUASARS; HIGH-REDSHIFT QUASARS; DEEP FIELD-SOUTH; ADVECTION-DOMINATED ACCRETION; EXTRAGALACTIC RADIO-SOURCES AB We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak quasar luminosity, and we determine this dependence using a large set of galaxy merger simulations varying galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions and obtain the evolution of the formation rate of quasars with peak luminosity, (n) over dot(L-peak, z). Quasars spend extended periods at luminosities well below peak, so (n) over dot(L-peak) has a maximum corresponding to the ``break'' in the observed luminosity function. From. n( Lpeak) and our simulations, we obtain self-consistent hard and soft X-ray and optical luminosity functions and predict many observables at multiple redshifts, including column density distributions of optical and X-ray samples, the luminosity function of broad-line quasars in X-ray samples and broad-line fraction versus luminosity, active BH mass functions, the distribution of Eddington ratios, the mass function of relic BHs and total BH mass density, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, without invoking ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 324 TC 913 Z9 914 U1 4 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2006 VL 163 IS 1 BP 1 EP 49 DI 10.1086/499298 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RO UT WOS:000236360000001 ER PT J AU Hopkins, PF Hernquist, L Cox, TJ Robertson, B Springel, V AF Hopkins, PF Hernquist, L Cox, TJ Robertson, B Springel, V TI Determining the properties and evolution of red galaxies from the quasar luminosity function SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE cosmology : theory; galaxies : active; galaxies : evolution; galaxies : nuclei; quasars : general ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; COLD DARK-MATTER; STAR-FORMATION HISTORIES; HIGH-REDSHIFT GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; FIELD ELLIPTIC GALAXIES; NEAR-INFRARED LUMINOSITY; LINE-STRENGTH GRADIENTS; RADIO-QUIET QUASARS AB We study the link between quasars and the red galaxy population using a model for self-regulated growth of super-massive black holes in gas-rich galaxy mergers. Using a model for quasar evolution motivated by hydrodynamic merger simulations, we deconvolve the observed quasar luminosity function at various redshifts to determine the rate of formation of black holes of a given final mass. Identifying quasar activity with the formation of spheroids in the framework of the merger hypothesis, this implies a corresponding rate of formation of spheroids with given properties as a function of redshift. This allows us to predict, for the red galaxy population, the distribution of galaxy velocity dispersions; mass functions; star formation rates; luminosity functions in many observed wave bands (NUV, U, B, V, R, I, J, H, K); the total red galaxy number, mass, and luminosity densities; color distributions as a function of magnitude and velocity dispersion for several different wave bands; the distribution of mass-to-light ratios versus mass; luminosity-size relations; and the typical ages and distribution of ages (formation redshifts) as a function of mass and luminosity. For each of these quantities, we predict the evolution from redshift z = 0-6. Each of our predictions agrees well with existing observations, without the addition of tunable parameters; the essential observational inputs come from the observed quasar luminosity function. These predictions are skewed by several orders of magnitude if we adopt simpler, traditional models of quasar lifetimes instead of the more complicated evolution implied by our simulations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 239 TC 117 Z9 117 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2006 VL 163 IS 1 BP 50 EP 79 DI 10.1086/499493 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RO UT WOS:000236360000002 ER PT J AU Rogel, AB Lugger, PM Cohn, HN Slavin, SD Grindlay, JE Zhao, P Hong, J AF Rogel, AB Lugger, PM Cohn, HN Slavin, SD Grindlay, JE Zhao, P Hong, J TI Three years of ChaMPlane northern field wiyn spectroscopy SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries : close; Galaxy : stellar content; novae, cataclysmic variables; quasars : general; stars : emission-line, Be; surveys ID HOLE BINARY A0620-00; DWARF FLARE STARS; CHROMOSPHERIC LINES; PHOTOMETRY; EMISSION; MASS; RED; NGC-1569; CLUSTERS; SPECTRA AB We present initial results of WIYN spectroscopic observations of selected objects detected in the Chandra Multiwavelength Plane (ChaMPlane) Survey in fields toward the Galactic anticenter. ChaMPlane is designed to identify low-luminosity X-ray sources, both accretion-powered and stellar coronal, in the Galaxy. It also includes a wide- field optical imaging Survey conducted with the NOAO Mosaic cameras to identify optical counterparts, as well as H alpha-selected objects in the similar to 5 times larger field. We report spectroscopic classifications for 1069 objects in Galactic anticenter (i.e., northern) fields, resulting in 612 type determinations. These include 5 new cataclysmic variables, 4 Be stars, 14 lithium-absorption stars, 182 stellar coronal sources (primarily dMe stars), and 30 new quasars. Bright optical counterparts of Chandra sources in this sample are most frequently dMe stars, whereas a majority of the faintest (R > 20. mag) spectroscopically classified Chandra source counterparts are quasars. The bulk of H alpha-selected sources appears to be roughly evenly divided between dMe stars and M stars at all magnitudes. C1 Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rogel, AB (reprint author), Indiana Univ, Dept Astron, Swain Hall W 319,727 E 3rd St, Bloomington, IN 47405 USA. EM abrogel@astro.indiana.edu NR 39 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2006 VL 163 IS 1 BP 160 EP 172 DI 10.1086/499433 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 026RO UT WOS:000236360000007 ER PT J AU Kajobe, R Roubik, DW AF Kajobe, R Roubik, DW TI Honey-making bee colony abundance and predation by apes and humans in a Uganda forest reserve SO BIOTROPICA LA English DT Article DE Apis; bee nest density; Bwindi-Uganda; chimpanzees; honey; Meliponini; predation; Pygmies ID LOWLAND DIPTEROCARP FORESTS; IMPENETRABLE-NATIONAL-PARK; STINGLESS BEES; NEST DENSITY; HYMENOPTERA; COMMUNITY; APIDAE; COMPETITION; DIVERSITY; MALAYSIA AB Honey-making bee colonies in Bwindi Impenetrable National Park were investigated with Batwa Pygmies locating 228 nests of Apis and five stingless bees (Meliponini). The relative importance of predation, food supply, nesting site, and elevation affecting abundance were studied for meliponines in particular. Nest predation and overall nest abundance had no correlation with elevation along a 1400 m gradient, nor did flowering phenology or pollen collection. Many suitable, large trees were unoccupied by bee nests. In 174 ha of forest plots, 2 Meliponula lendliana, 13 M. nebulata, 16 M. ferruginea, 16 M. bocandei, and 20 Apis mellifera adansonii nests occurred, suggesting a habitat-wide density of 39 nests/km(2). Compared to other studies, Ugandan Meliponini were uncommon (0.27 colonies/ha, tropical mean = 1.9/ha), while Apis mellifera was numerous (0.12 nests/ha, tropical mean = 0.06/ha), despite park policy allowing humans to exploit Apis. Meliponine colony mortality from predators averaged 12 percent/yr and those near ground were most affected. Tool-using humans and chimpanzees caused 82 percent of stingless bee nest predation. Selective factors affecting nest heights and habit may include auditory hunting by predators for buzzing bees, and indirect mutualists such as termites that leave potential nesting cavities. Mobility and free-nesting by honey bee colonies should enable rapid community recovery after mortality, especially in parks where human honey hunting is frequent, compared to sedentary and nest-site-bound Meliponini. C1 Fac Biol, Dept Behav Biol, Trop Bee Res Unit, NL-3508 TB Utrecht, Netherlands. Smithsonian Trop Res Inst, Balboa, Panama. RP Kajobe, R (reprint author), Makerere Univ, Fac Forestry & Nat Conservat, POB 7062, Kampala, Uganda. EM kajobe@forest.mak.ac.ug NR 48 TC 27 Z9 28 U1 0 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2006 VL 38 IS 2 BP 210 EP 218 DI 10.1111/j.1744-7429.2006.00126.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 010RA UT WOS:000235210600008 ER PT J AU Gerwing, JJ Schnitzer, SA Burnham, RJ Bongers, F Chave, J DeWalt, SJ Ewango, CEN Foster, R Kenfack, D Martinez-Ramos, M Parren, M Parthasarathy, N Perez-Salicrup, DR Putz, FE Thomas, DW AF Gerwing, JJ Schnitzer, SA Burnham, RJ Bongers, F Chave, J DeWalt, SJ Ewango, CEN Foster, R Kenfack, D Martinez-Ramos, M Parren, M Parthasarathy, N Perez-Salicrup, DR Putz, FE Thomas, DW TI A standard protocol for liana censuses SO BIOTROPICA LA English DT Article DE biodiversity; biomass; census methods; inventory; lianas ID TROPICAL RAIN-FOREST; BARRO-COLORADO-ISLAND; LOWLAND FOREST; STEM DIAMETER; WET FOREST; DIVERSITY; ABUNDANCE; GROWTH; BIOMASS; PANAMA AB A recent increase in published studies of lianas has been paralleled by a proliferation of protocols for censusing lianas. This article seeks to increase uniformity in liana inventories by providing specific recommendations for the determination of which taxa to include, the location of diameter measurement points on individual stems, the setting of minimum stem diameter cutoffs, the treatment of multiple-stemmed and rooted clonal groups, and the measurement of noncylindrical stems. Use of more uniform liana censusing protocols may facilitate comparison of independently collected data sets and further our understanding of global patterns in liana abundance, diversity, biomass, and dynamics. C1 Portland State Univ, Univ Studies, Portland, OR 97207 USA. Inst Homem & Meio Ambiente Amazonia IMAZON, Belem, Para, Brazil. Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. Wageningen Univ, Dept Environm Sci, Forest Ecol & Forest Management Grp, Wageningen, Netherlands. CNRS, Lab Evolut & Divers Biol, Toulouse, France. Univ Toulouse 3, F-31062 Toulouse, France. Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Field Museum, Environm & Conservat Programs, Chicago, IL 60605 USA. Missouri Bot Garden, Dept 43, St Louis, MO 63110 USA. Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58089, Michoacan, Mexico. Forestry Commiss, Validat Legal Timber Programme, Accra, Ghana. Pondicherry Univ, Dept Ecol & Environm Sci, Pondicherry, India. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Ancon, Panama. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. RP Gerwing, JJ (reprint author), Portland State Univ, Univ Studies, POB 751, Portland, OR 97207 USA. EM jgerwing@pdx.edu OI Schnitzer, Stefan/0000-0002-2715-9455 NR 44 TC 91 Z9 103 U1 3 U2 29 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2006 VL 38 IS 2 BP 256 EP 261 DI 10.1111/j.1744-7429.2006.00134.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 010RA UT WOS:000235210600012 ER PT J AU Staines, CL Staines, SL AF Staines, CL Staines, SL TI Additional eastern US records of the introduced leaf beetle Chrysolina quadrigemina (Suffrian) (Coleoptera : Chrysomelidae) SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu NR 2 TC 1 Z9 1 U1 0 U2 0 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD MAR PY 2006 VL 60 IS 1 BP 72 EP 72 DI 10.1649/880.1 PG 1 WC Entomology SC Entomology GA 034MS UT WOS:000236933700015 ER PT J AU Howard, FW Hodges, GS Gates, MW AF Howard, FW Hodges, GS Gates, MW TI First report of conchaspis cordiae (Hemiptera : Conchaspididae) in Florida and the United States SO FLORIDA ENTOMOLOGIST LA English DT Editorial Material C1 Univ Florida, Ft Lauderdale Res & Educ Ctr, IFAS, Ft Lauderdale, FL 33314 USA. Florida Dept Agr & Consumer Serv, Div Plant Ind, Florida State Collect Arthropods, Gainesville, FL 32614 USA. ARS, USDA, PSI,SEL, Smithsonian Inst,NMNH, Washington, DC 20013 USA. RP Howard, FW (reprint author), Univ Florida, Ft Lauderdale Res & Educ Ctr, IFAS, 3205 Coll Ave, Ft Lauderdale, FL 33314 USA. NR 5 TC 0 Z9 0 U1 1 U2 1 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD MAR PY 2006 VL 89 IS 1 BP 102 EP 104 DI 10.1653/0015-4040(2006)89[102:FROCCH]2.0.CO;2 PG 3 WC Entomology SC Entomology GA 025GC UT WOS:000236252300021 ER PT J AU Kirshenblatt-Gimblett, B Hufford, M Hunt, M Zeitlin, S AF Kirshenblatt-Gimblett, Barbara Hufford, Mary Hunt, Marjorie Zeitlin, Stepe TI The grand generation: Folklore and the culture of aging SO GENERATIONS-JOURNAL OF THE AMERICAN SOCIETY ON AGING LA English DT Article C1 NYU, New York, NY 10011 USA. Univ Penn, Ctr Folklore & Ethnog, Philadelphia, PA 19104 USA. Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. CityLore, New York, NY USA. RP Kirshenblatt-Gimblett, B (reprint author), NYU, New York, NY 10011 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC AGING PI SAN FRANCISCO PA 833 MARKET ST, STE 511, SAN FRANCISCO, CA 94103-1824 USA SN 0738-7806 J9 GENERATIONS JI Generations-J. Am. Soc. Aging PD SPR PY 2006 VL 30 IS 1 BP 32 EP 37 PG 6 WC Gerontology SC Geriatrics & Gerontology GA V44EF UT WOS:000202985300008 ER PT J AU McMillan, ME Heller, PL Wing, SL AF McMillan, ME Heller, PL Wing, SL TI History and causes of post-Laramide relief in the Rocky Mountain orogenic plateau SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Review DE Cenozoic; tectonic uplift; climate change; incision; Rocky Mountains; Colorado Plateau ID WESTERN UNITED-STATES; LATE CENOZOIC UPLIFT; COLORADO PLATEAU; CLIMATE-CHANGE; EROSION RATES; NORTH-AMERICA; GREAT-PLAINS; CONTINENTAL INTERIORS; PLIOCENE UPLIFT; BOUSE FORMATION AB The Rocky Mountain orogenic plateau has the highest mean elevation and topographic relief in the contiguous United States. The mean altitude exceeds 2 km above sea level and relief increases front 30 in in the river valleys of the Great Plains to more than 1.6 km deep in the canyons and basins of the Rocky Mountains and Colorado Plateau. Despite over a century of study, the timing and causes of elevation gain and incision in the region are unclear. Post-Laramide development of relief is thought to either result from tectonic activity or climatic change. Interpretation of which of these causes dominated is based upon reconstruction of datums developed from, and supported by, paleoelevation proxies and interpretations of landscape incision. Here we reconstruct a datum surface against which regional incision can be measured in order to evaluate late Cenozoic tectonic and climatic influences. The distribution, magnitude, and timing of post-Laramide basin filling and subsequent erosion are constrained by depositional remnants, topographic markers, and other indicators across the region. We suggest that post-Laramide basin filling resulted from slow subsidence during Oligocene to Miocene time. Incision into this basin fill surface began in late Miocene time and continues today. The pattern of incision is consistent with control by localized extensional tectonism superimposed upon regional domal surface uplift. Localized extension is associated with the projection of the Rio Grande Rift into the central Rockies, and the domal uplift generally coincides with the position of buoyant mantle anomalies interpreted at depth. If the magnitudes of incision directly reflect magnitudes of surface elevation gain, they are less than can be resolved by existing palcoelevation proxy methods. In addition, the combination of post-Laramide subsidence followed by regional surface uplift reduces the net magnitude of surface elevation change since Laramide time. C1 Univ Arkansas, Dept Earth Sci, Little Rock, AR 72204 USA. Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP McMillan, ME (reprint author), Univ Arkansas, Dept Earth Sci, 2801 S Univ Ave, Little Rock, AR 72204 USA. EM memcmillan@ualr.edu; heller@uwyo.edu; wing.scott@nmnh.si.edu OI Wing, Scott/0000-0002-2954-8905 NR 127 TC 72 Z9 75 U1 0 U2 16 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAR-APR PY 2006 VL 118 IS 3-4 BP 393 EP 405 DI 10.1130/B25715.1 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 021DC UT WOS:000235962700010 ER PT J AU Hall, MC Stiling, P Moon, DC Drake, BG Hunter, MD AF Hall, MC Stiling, P Moon, DC Drake, BG Hunter, MD TI Elevated CO2 increases the long-term decomposition rate of Quercus myrtifolia leaf litter SO GLOBAL CHANGE BIOLOGY LA English DT Article DE ammonium; decomposition; elevated CO2; herbivory; Kennedy space center; litter quality; mass loss; nitrate; Quercus myrtifolia ID SCRUB-OAK ECOSYSTEM; OPEN-TOP CHAMBERS; ATMOSPHERIC CO2; CARBON-DIOXIDE; GYPSY-MOTH; TALLGRASS PRAIRIE; HERBIVORE DAMAGE; QUALITY; NITROGEN; FOREST AB Decomposition of Quercus myrtifolia leaf litter in a Florida scrub oak community was followed for 3 years in two separate experiments. In the first experiment, we examined the effects CO2 and herbivore damage on litter quality and subsequent decomposition. Undamaged, chewed and mined litter generated under ambient and elevated (ambient+350 ppm V) CO2 was allowed to decompose under ambient conditions for 3 years. Initial litter chemistry indicated that CO2 levels had minor effects on litter quality. Litter damaged by leaf miners had higher initial concentrations of condensed tannins and nitrogen (N) and lower concentrations of hemicellulose and C : N ratios compared with undamaged and chewed litter. Despite variation in litter quality associated with CO2, herbivory, and their interaction, there was no subsequent effect on rates of decomposition under ambient atmospheric conditions. In the second experiment, we examined the effects of source (ambient and elevated) of litter and decomposition site (ambient and elevated) on litter decomposition and N dynamics. Litter was not separated by damage type. The litter from both elevated and ambient CO2 was then decomposed in both elevated and ambient CO2 chambers. Initial litter chemistry indicated that concentrations of carbon (C), hemicellulose, and lignin were higher in litter from elevated than ambient CO2 chambers. Despite differences in C and fiber concentrations, litter from ambient and elevated CO2 decomposed at comparable rates. However, the atmosphere in which the decomposition took place resulted in significant differences in rates of decomposition. Litter decomposing under elevated CO2 decomposed more rapidly than litter under ambient CO2, and exhibited higher rates of mineral N accumulation. The results suggest that the atmospheric conditions during the decomposition process have a greater impact on rates of decomposition and N cycling than do the atmospheric conditions under which the foliage was produced. C1 Univ Georgia, Inst Ecol, Athens, GA 30602 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hunter, MD (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. EM mdhunter@umich.edu NR 50 TC 13 Z9 20 U1 1 U2 17 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2006 VL 12 IS 3 BP 568 EP 577 DI 10.1111/h.1365-2486.2006.01119.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 021YY UT WOS:000236023000014 ER PT J AU Vari, RP Chang, F AF Vari, RP Chang, F TI Cyphocharax derhami, a new species (Ostariophysi : Characiformes : Curimatidae) from northeastern Peru SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS LA English DT Article AB Cyphocharax derhami, new species, is described from two localities in the northeastern portion of Peru. This species can be distinguished from its congeners by a combination of morphometric, meristic, and pigmentary features, most obviously the distinct bar of dark pigmentation extending posteroventrally from the rear of the orbit to the posterior margin of the opercle. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. Univ Nacl Mayor San Marcos, Museum Nat Hist, Dept Ictiol, Lima 14, Peru. RP Vari, RP (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Div Fishes, MRC-159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu NR 4 TC 8 Z9 8 U1 0 U2 0 PU VERLAG DR. FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0936-9902 J9 ICHTHYOL EXPLOR FRES JI Ichthyol. Explor. Freshw. PD MAR PY 2006 VL 17 IS 1 BP 93 EP 96 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 018LC UT WOS:000235764700009 ER PT J AU Murray, S Sanchez, C Bronson, E Harris, C AF Murray, S Sanchez, C Bronson, E Harris, C TI Diagnostic imaging in veterinary dental practice SO JAVMA-JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Editorial Material ID CHINCHILLAS; ODONTOMA; DISEASE C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. Wildlife Ctr Virginia, Waynesboro, VA 22980 USA. RP Murray, S (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 9 TC 2 Z9 2 U1 0 U2 1 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0003-1488 J9 JAVMA-J AM VET MED A JI JAVMA-J. Am. Vet. Med. Assoc. PD MAR 1 PY 2006 VL 228 IS 5 BP 697 EP 698 DI 10.2460/javma.228.5.697 PG 2 WC Veterinary Sciences SC Veterinary Sciences GA 021IP UT WOS:000235977200029 PM 16506929 ER PT J AU Pisano, DA AF Pisano, Dominick A. TI Flying down to Rio: Hollywood, tourists, and Yankee clippers. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review 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 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2006 VL 92 IS 4 BP 1473 EP 1474 PG 2 WC History SC History GA 082JJ UT WOS:000240382400093 ER PT J AU Austin, D Bowen, WD McMillan, JI Boness, DJ AF Austin, D Bowen, WD McMillan, JI Boness, DJ TI Stomach temperature telemetry reveals temporal patterns of foraging success in a free-ranging marine mammal SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE distribution of feeding; grey seals; meal frequency; predators; sex differences ID SEALS HALICHOERUS-GRYPUS; DIMORPHIC CAPITAL BREEDER; SEX-DIFFERENCES; GREY SEAL; SPLITTING BEHAVIOR; FEEDING-BEHAVIOR; DIVING BEHAVIOR; PHOCA-VITULINA; SCOTIAN SHELF; FOOD-INTAKE AB We studied feeding frequency in free-ranging grey seals using stomach temperature telemetry to test if previously reported sex differences in the diving, movement and diet were reflected in the temporal pattern of foraging success. Data were retrieved from 21 of 32 grey seals from 1999 to 2001, totalling 343 days and 555 feeding events, with individual record length varying from 2 to 40 days (mean: 16.33 +/- 2.67 days/seal). Seals fed on 57.8 +/- 6.46% of days sampled and had an average of 1.7 +/- 0.26 meals per day, but individual variability was apparent in the temporal distribution of feeding as evidenced by high coefficients of variation (coefficient of variation = 69.0%). Bout analysis of non-feeding intervals of six grey seals suggests that feeding intervals of individuals were varied and probably reflect differences in prey availability. Grey seals tended to have many single feeding events with long periods separating each event, as would be expected for a large carnivore with a batch-reactor digestive system. We found significant sex differences in the temporal distribution of feeding. The number of feeding events per day was greater in males (2.2 +/- 0.4 vs. 1.0 +/- 0.2), as was time associated with feeding per day (56.6 +/- 5.8 min vs. 43.9 +/- 9.4 min). The number of feeding events varied with time of day with the least number occurring during dawn. Feeding event size differed significantly by time of day, with greater meal sizes during the dawn and the smallest meals during the night. The length of time between meals increased with the size of the previous meal, and was significantly less in males (541.4 +/- 63.5 min) than in females (1092.6 +/- 169.9 min). These results provide new insight into the basis of sex differences in diving and diet in this large size-dimorphic marine predator. C1 Dalhousie Univ, Dept Biol, Halifax, NS B2H 4J1, Canada. Bedford Inst Oceanog, Marine Fish Div, Dept Fisheries & Oceans, Dartmouth, NS B2Y 4A2, Canada. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. RP Austin, D (reprint author), Univ Calif Santa Cruz, Long Marine Lab, Santa Cruz, CA 95060 USA. EM austin@biology.ucsc.edu RI Bowen, William/D-2758-2012 NR 80 TC 59 Z9 60 U1 2 U2 13 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8790 J9 J ANIM ECOL JI J. Anim. Ecol. PD MAR PY 2006 VL 75 IS 2 BP 408 EP 420 DI 10.1111/j.1365-2656.2006.01057.x PG 13 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 027AJ UT WOS:000236384700010 PM 16637994 ER PT J AU Adams, RM AF Adams, RM TI Myths of the archaic state: Evolution of the earliest cities, states, and civilizations. SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 Univ Calif San Diego, San Diego, CA 92103 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Adams, RM (reprint author), Univ Calif San Diego, San Diego, CA 92103 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO PI ALBUQUERQUE PA DEPT ANTHROPOLOGY, ALBUQUERQUE, NM 87131-1561 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SPR PY 2006 VL 62 IS 1 BP 154 EP 155 PG 2 WC Anthropology SC Anthropology GA 026ZE UT WOS:000236381300029 ER PT J AU Stanley, JD Bernasconi, MP AF Stanley, JD Bernasconi, MP TI Holocene depositional patterns and evolution in Alexandria's Eastern Harbor, Egypt SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Alexandria; ancient parts; biofacies; correlation; geoarcheology; Heptastadion; hiatus; human impact; kurkar; Ptolomies; radiocarbon dates; sediment failure; stratigraphy; transport processes; vibracores ID NILE DELTA; LATE QUATERNARY; NORTHWESTERN EGYPT; SEDIMENTS; CIRCULATION; DESTRUCTION; INTERFACE; REGION; ISRAEL; COAST AB This investigation focuses oil sedimentological attributes and the litho- and chronostratigraphic framework of Holocene sediment core sections recovered in Alexandria's Eastern Harbor in Egypt, for many centuries the major port in the southeast Mediterranean. Holocene sediment trapped in the harbor, formed of marine calcareous sand, muddy sand, and mud, are examined to define major depositional patterns that developed before and after expansion of Alexandria in the 4th Century BC. Petrologic and radiocarbon data indicate that the harbor formed between two Pleistocene carbonate sandstone (kurkar) coastal ridges and was flooded by seawater during the transgression at about 8000 years before present (BP). Sediments accumulated at an average rate of 1-3 mm/y largely by wave- and wind-driven currents driving material from the Egyptian shelf into the high-energy basin. The association of distinct biological components, failed slump-like sediment strata, and important hiatuses (time gaps) record the episodic influence of powerful events, such as large storm surges, seismic tremors, and tsunamis. These events likely transported marine biota and sediment from the kurkar ridge and inner shelf north of the harbor and also eroded and displaced substantial amounts of older deposits laterally within the basin. In addition to natural processes, the influence of human activity is detected in harbor sediments after similar to 2400 years BP, following development of Alexandria by the Ptolomies and their successors, the Romans. Among important components in cores are artifacts and lithoclasts. The development of important mud-rich deposits from similar to 2200 to 1800 years BP is attributed in part to construction of the Heptastadion, the large causeway and aquaduct system built to connect Alexandria with Pharos Island to the north. Structures such as breakwaters have modified sedimentation patterns but do not fully protect the quasi-closed harbor. Ongoing geoarcheological investigations hold promise to more precisely distinguish effects of natural processes from those of human-related activities. C1 Smithsonian Inst, Geoarchaeol Program, Paleobiol NMNH E205, Washington, DC 20013 USA. Univ Calabria, Dipartimento Sci Terra, I-87036 Arcavacata Di Rende, Consenza, Italy. RP Stanley, JD (reprint author), Smithsonian Inst, Geoarchaeol Program, Paleobiol NMNH E205, Washington, DC 20013 USA. EM stanley.daniel@NMNH.SI.edu NR 40 TC 14 Z9 14 U1 0 U2 7 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD MAR PY 2006 VL 22 IS 2 BP 283 EP 297 DI 10.2112/04-0348.1 PG 15 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 026KW UT WOS:000236338800003 ER PT J AU Brandley, MC Wynn, A de Queiroz, K AF Brandley, MC Wynn, A de Queiroz, K TI Karyotype and relationships of anolis desechensis SO JOURNAL OF HERPETOLOGY LA English DT Article ID CHROMOSOME; IGUANIDAE; SAURIA AB We determined the karyotype of Anolis desechensis and compared it with the known karyotypes of other members of the Anolis cristatellus series. The diploid (2N) number of chromosomes of two male A. desechensis was 27, with six pairs of large metacentric macrochromosomes, six pairs of microchromosomes of gradually decreasing size, and sex chromosome heteromorphism (three sex chromosomes, X1X2Y). This chromosome complement is identical to that of A. cristatellus and A. scriptus, thus providing additional evidence of a close relationship to these taxa. The evolution of chromosome number within the cristatellus series appears to have involved minimal homoplasy and therefore contains useful phylogenetic information. C1 Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Brandley, MC (reprint author), Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. EM brandley@berkeley.edu NR 15 TC 4 Z9 4 U1 0 U2 1 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD MAR PY 2006 VL 40 IS 1 BP 136 EP 139 DI 10.1670/98-05N.1 PG 4 WC Zoology SC Zoology GA 031OS UT WOS:000236714500021 ER PT J AU Medina, A Scelzo, MA Tudge, CC AF Medina, A Scelzo, MA Tudge, CC TI Spermatozoal ultrastructure in three Atlantic solenocerid shrimps (Decapoda, Dendrobranchiata) SO JOURNAL OF MORPHOLOGY LA English DT Article DE sperm ultrastructure; Solenocera membranacea; Solenocera africana; Pleoticus muelleri; Crustacea; Dendrobranchiata; Solenoceridae ID ARISTEUS-ANTENNATUS; PENAEUS-JAPONICUS; SICYONIA-INGENTIS; SPERM; CRUSTACEA; SPERMIOGENESIS; PENAEIDAE AB The spermatozoal ultrastructure in three solenocerid shrimps (Solenocera membranacea, S. africana, and Pleoticus muelleri) from different Atlantic locations was examined with the aim of increasing understanding of the phylogenetic relationships in the Dendrobranchiata. A considerable structural similarity between the sperm of these species and those of penaeid shrimps supports a close affinity between the Penaeidae and Solenoceridae. However, significant differences in the sperm morphology of the previously investigated sicyoniids (namely, a greater complexity of the acrosomal complex) suggest evolutionary separation of the Sicyoniidae from the assemblage Penaeidae-Solenoceridae. Two ultrastructural features distinguish the spermatozoa of the three studied solenocerids from penaeid sperm: 1) separation of the plasma and acrosome membranes at the base of the spike and anterior region of the cap, and 2) asymmetry of the acrosomal cap, which appears to be a synapomorphy of the group. No striking ultrastructural differences were found between the spermatozoa of the closely related species S. membranacea and S. africana, whereas a great number of morphological differences separate the spermatozoa of Pleoticus from those of Solenocera (e.g., shape of the acrosomal cap, structural arrangement of the contents of the whole acrosome vesicle, thickness and distribution of the cytoplasm, and external shape of the spike). C1 Fac Ciencias Mar & Ambientales, Dept Biol, E-11510 Cadiz, Spain. Univ Nacl Mar del Plata, CONICET, FCEyN, Dept Ciencias Marinas, Mar Del Plata, Argentina. American Univ, Dept Invertebrate Zool, MRC 163, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20016 USA. American Univ, Dept Biol, Washington, DC 20016 USA. RP Medina, A (reprint author), Fac Ciencias Mar & Ambientales, Dept Biol, Avda Republ Saharaui,S-N, E-11510 Cadiz, Spain. EM antonio.medina@uca.es RI Medina, Antonio/A-1624-2008 OI Medina, Antonio/0000-0001-5609-3574 NR 28 TC 6 Z9 7 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD MAR PY 2006 VL 267 IS 3 BP 300 EP 307 DI 10.1002/jmor.10404 PG 8 WC Anatomy & Morphology SC Anatomy & Morphology GA 013ME UT WOS:000235412600004 PM 16323220 ER PT J AU Pecchio, M Solis, PN Lopez-Perez, JL Vasquez, Y Rodriguez, N Olmedo, D Correa, M San Feliciano, A Gupta, MP AF Pecchio, M Solis, PN Lopez-Perez, JL Vasquez, Y Rodriguez, N Olmedo, D Correa, M San Feliciano, A Gupta, MP TI Cytotoxic and antimicrobial benzophenones from the leaves of Tovomita longifolia SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID BRAZILIAN GUTTIFERAE; CONSTITUENTS; CHEMISTRY; PLANTS AB Bioassay-guided fractionation of the chloroform and ethanol extracts of Tovomita longifolia leaves using cytotoxic and antimicrobial assays resulted in the isolation of four new benzophenones, (E)-3-(2-hydroxy-7-methyl-3-methyleneoct-6-enyl)-2,4,6-trihydroxybenzophenone (1), (E)-3-(6-hydroxy-3,7-dimethylocta-2,7-dienyl)-2,4,6-trihydroxybenzophenone (2), 8-benzoyl-2-(4-methylpenten-3-yl)chromane-3,5,7-triol (3), and 5-benzoyl-1,1,4a-trimethyl-2,3,4,4a,9,9a-hexahydro-1H-xanthene-6,8-diol (4), and two known benzophenones, 4-geranyloxy-2,6-dihydroxybenzophenone (5) and 3-geranyl-2,4,6-trihydroxybenzophenone (6). The structures of 1-4 were established by spectroscopic means and by molecular modeling calculations. Compounds 1 and 3-5 demonstrated cytotoxic activities against breast (MCF-7), central nervous system (SF-268), and lung (H-460) human cancer cell lines, while compounds 3-6 showed antimicrobial activity against Klebsiella pneumoniae, Mycobacterium smegmatis, Pseudomonas aeruginosa, Salmonella gallinarum, and Staphylococcus aureus. C1 Univ Panama, Fac Farm, Ctr Invest Farmacognost Flora Panamena, Panama City, Panama. Univ Salamanca, Fac Farm, Dept Quim Farmaceut, Salamanca, Spain. Herbario Univ Panama, Panama City, Panama. Smithsonian Trop Res Inst, Panama City, Panama. RP Gupta, MP (reprint author), Univ Panama, Fac Farm, Ctr Invest Farmacognost Flora Panamena, Panama City, Panama. EM cytedqff@ancon.up.ac.pa RI San Feliciano, Arturo/K-9603-2014; Lopez-Perez, Jose/M-8763-2013; OI San Feliciano, Arturo/0000-0002-0578-0611; Lopez-Perez, Jose/0000-0002-3728-7602; Gupta, Mahabir/0000-0002-9302-7864 NR 21 TC 38 Z9 38 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD MAR PY 2006 VL 69 IS 3 BP 410 EP 413 DI 10.1021/np050338c PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 028OK UT WOS:000236497400024 PM 16562847 ER PT J AU Herrera-Cubilla, A Dick, MH Sanner, J Jackson, JBC AF Herrera-Cubilla, A Dick, MH Sanner, J Jackson, JBC TI Neogene Cupuladriidae of tropical America. I: Taxonomy of recent Cupuladria from opposite sides of the Isthmus of Panama SO JOURNAL OF PALEONTOLOGY LA English DT Article ID REEF CORALS; BRYOZOA; PHYLOGENY; HISTORY; TEMPO AB We used up to 28 morphological characters to discriminate and describe species of the genus Cupuladria based on entire colony specimens collected from both coasts of the Isthmus of Panama. The characters included a combination of zooidal features traditionally used in cheilostome taxonomy and nontraditional characters Such as colony size, shape, and an index of calcification of the colony, as well as the size of the basal sectors and their number of pores. Species were discriminated by a series of repeated multivariate cluster and discriminant analyses until the majority of specimens were assigned to their putative species with high statistical confidence. Nontraditional characters contributed significantly to the power of the analyses. Colonies fell into two highly distinct groups most clearly recognized by the presence or absence of vicarious avicularia, which agrees well with previous molecular genetic analyses. Further analyses of each of these two groups considered separately resulted in the discrimination of eight species. These include two previously described Caribbean species, C. biporosa Canu and Bassler, 1919 and C. surinamensis Cadde, 1975, and six new species: C. multesima, C. incognita, C. cheethami, and C. panamensis from the Caribbean, and C. pacificiensis and C. exfragminis from the eastern Pacific. There was also good correspondence between major clades within these morphologically defined groups and the previous molecular analysis, although 20% of the specimens Could not be distinguished from their cognate ("geminate") species from the opposite ocean. The high ratio Of undescribed to described species and higher diversity in the Caribbean than eastern Pacific agree well with newly described patterns from other cheilostome genera based oil similar analyses. Quantitative morphometric Studies are-essential to Study biologically meaningful patterns of cheilostome speciation and macroevolution in the fossil record. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. Hokkaido Univ, Grad Sch Sci, COE Program Neo Sci Nat Hist, Sapporo, Hokkaido 0600810, Japan. Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Herrera-Cubilla, A (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Box 2072, Balboa, Panama. EM herreraa@ancon.si.edu; mhdick@nature.sci.hokudai.ac.jp; SannerJ@si.edu; jbcj@used.edu RI Dick, Matthew/E-1327-2012 NR 48 TC 16 Z9 16 U1 0 U2 3 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 MAR PY 2006 VL 80 IS 2 BP 245 EP 263 DI 10.1666/0022-3360(2006)080[0245:NCOTAI]2.0.CO;2 PG 19 WC Paleontology SC Paleontology GA 017CA UT WOS:000235670500004 ER PT J AU Johnson, KG Kirby, MX AF Johnson, KG Kirby, MX TI The emperador limestone rediscovered: Early Miocene corals from the Culebra Formation, Panama SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CARIBBEAN REEF CORALS; MIDDLE MIOCENE; EXTINCTION; NEOGENE; DIVERSITY AB Caribbean reefs underwent significant biotic change during the Late Oligocene and Early Miocene. This was a critical time in the evolution of the modern Caribbean fauna characterized by increasing endemisin resulting from regional extinction of lineages that survive in the modern Indo-Pacific. All understanding of the dynamics and potential causes of the Oligocene/Miocene transition, however, is hampered by the relative lack of well-preserved Oligocene to early Miocene coral faunas in the Caribbean. Here we examine new exposures in the Culebra Formation of Panama that contain a well-preserved coral fauna of Early Miocene age. Taxonomic, stratigraphic, and paleoecologic study of the Culebra Formation exposed along the Gaillard Cut of the Panama Canal allows LIS to infer the paleoenvironments and reef coral communities front the Panama Canal Basin during this critical interval. The Culebra Formation consists of a deepening upward Sequence with shallow-lagoon sediments at the base, overlain by fringing reef facics in the middle of the section, and open-shelf to bathyal facies at the top of the section. We recovered 31 species of reef corals from a combination of now and old collections. Comparison of our collections with other Late Oligocene to Middle Miocene reef coral assemblages confirms that there was a major faunal turnover after deposition of the Upper Oligocene Antigua Formation. This turnover consisted of a large number of extinctions followed by all increase(] rate of first occurrences so that regional diversity did not change appreciably. Improved stratigraphic resolution at this and other Caribbean localities is required to understand fully the dynamics of change during the Oligocene/ Miocene transition. C1 Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. RP Kirby, MX (reprint author), Nat Hist Museum, Dept Palaeontol, Cromwell Rd, London SW7 5BD, England. EM K.Johnson@nhm.ac.uk NR 59 TC 15 Z9 18 U1 0 U2 0 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 MAR PY 2006 VL 80 IS 2 BP 283 EP 293 DI 10.1666/0022-3360(2006)080[0283:TELREM]2.0.CO;2 PG 11 WC Paleontology SC Paleontology GA 017CA UT WOS:000235670500007 ER PT J AU Simeckova, M Jacquemart, D Rothman, LS Gamache, RR Goldman, A AF Simeckova, M Jacquemart, D Rothman, LS Gamache, RR Goldman, A TI Einstein A-coefficients and statistical weights for molecular absorption transitions in the HITRAN database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Einstein A-coefficient; statistical weight; spectroscopic database; atmospheric database; HITRAN ID INTERNAL PARTITION SUMS; ENERGY-LEVELS; SPECTROSCOPIC DATABASE; LINE-INTENSITIES; MU-M; EDITION; BANDS; CLASSIFICATION; (C2H2)-C-12; PARAMETERS AB This paper describes the calculation of the statistical weights and the Einstein A-coefficients for the 39 molecules and their associated isotopologues/isotopomers currently present in the line-by-line portion of the HITRAN database. Calculation of the Einstein A-coefficients was carried out using the HITRAN line intensities and the necessary statistical weights. The Einstein A-coefficient and the statistical weights of the upper and lower levels of the transition were added in the new format of the line parameters for the most recent edition of the HITRAN database. (c) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Mass, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 40 TC 61 Z9 65 U1 4 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2006 VL 98 IS 1 BP 130 EP 155 DI 10.1016/j.jqrst.2005.07.003 PG 26 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 998HP UT WOS:000234309600013 ER PT J AU Baron-Szabo, RC AF Baron-Szabo, RC TI Corals of the K/T-boundary: Scleractinian corals of the suborders Astrocoeniina, Faviina, Rhipidogyrina and Amphiastraeina SO JOURNAL OF SYSTEMATIC PALAEONTOLOGY LA English DT Review DE Maastrichtian; Paleocene; K-T; taxonomy; stratigraphical and geographical distribution ID REEF; TERTIARY AB This taxonomic review of the scleractinian corals of the Maastrichtian and Paleocene period focuses on the scleractinian suborders Astrocoeniina, Faviina, Rhipidogyrina and Amphiastraeina. This, the first extensive compilation of coral species of the K/T (Cretaceous/Tertiary) boundary, deals with more than 2500 records Of 550 nominal taxa. In addition to the re-examination and re-evaluation of described forms, this study also includes the first description of the largest Maastrichtian coral assemblage known (consisting of about 4000 specimens from Jamaica), as well as new material from the Campanian-Maastrichtian of Argentina, Lower Maastrichtian of Mexico (Cerralvo), and the Paleocene of Austria (Kambuhel-Kalke). A diagnosis is provided for each species, as welt as for each higher-level taxonomic category and issues concerning taxonomic assignment are discussed in detail. The descriptions are accompanied by illustrations of representatives of each species and, in many cases, include illustrations of type or original material. Also included is the first comprehensive overview of the stratigraphical and geographical ranges of each taxon. In the four suborders evaluated in this paper, 123 valid species can be reliably documented as occurring in the Maastrichtian and/or the Pateocene. The largest number of species is in the suborders Faviina and Astrocoeniina. In the Faviina 62 valid species are known from the Maastrichtian, of which 35 (56.5%) crossed the K/T-boundary, while in the Paleocene 14 new species appeared. In the Astrocoeniina 18 valid species occurred in the Maastrichtian, eight of which (44.4%) crossed the K/T-boundary and 16 new species appeared in the Paleocene. Only eight species of Rhipidogyrina and five species of Amphiastraeina occurred in the Maastrichtian and although two amphiastraeinid made it into the Paleocene, only one of the rhipidogyrinids crossed the K/T-boundary. No new species of Amphiastraeina appeared in the Paleocene. According to this revision on the genus level 44 out of the 65 genera crossed the K/T-boundary, which is 67.7% (12 genera went extinct, 9 genera have their first occurrence in the Paleocene). In comparison to previous estimates this result (generic extinction of around 32%) represents the best estimation for scleractinian corals at present and corresponds to recently reported results of other macroinvertebrate groups after taxonomic revision (e.g. echinoids). C1 Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Res Inst Senckenberg, D-60325 Frankfurt, Germany. RP Baron-Szabo, RC (reprint author), Smithsonian Inst, Dept Invertebrate Zool, W-329,MRC-163, Washington, DC 20013 USA. NR 321 TC 29 Z9 33 U1 1 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1477-2019 J9 J SYST PALAEONTOL JI J. Syst. Palaeontol. PD MAR PY 2006 VL 4 IS 1 BP 1 EP 108 DI 10.1017/S1477201905001689 PG 108 WC Evolutionary Biology; Paleontology SC Evolutionary Biology; Paleontology GA 022XD UT WOS:000236088500001 ER PT J AU Geier, K AF Geier, Katharina TI A technical study of arctic pigments and paint on two 19th-century Yup'ik masks SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB This article presents the results of a technical study of the paint layers on two 19th-century Yup'ik masks and raw pigments from the Smithsonian Institution's National Museum of Natural History. The materials and techniques of manufacture were investigated to inform decisionmaking regarding optimal conservation and restoration. Information on materials and methods used by the Yup'ik is reviewed, and results of analysis are described. The paint samples taken from the masks and from raw pigments show that both are comprised mainly of natural minerals and earth colors. One of the black raw pigments was found to be a mixture of carbon particles, heated vegetable oils and resin, and clay The pigments were applied without detectable organic binders, and their application is more complex than is described in available literature and ethnographic reports. C1 Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Museum Support Ctr, Suitland, MD 20746 USA. RP Geier, K (reprint author), Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Museum Support Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 USA SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SPR PY 2006 VL 45 IS 1 BP 17 EP 30 PG 14 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 091FW UT WOS:000241013300002 ER PT J AU Langley, HD AF Langley, HD TI Stephen Decatur: A life most bold and daring. SO JOURNAL OF THE EARLY REPUBLIC LA English DT Book Review C1 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 HISTORIANS EARLY AMERICAN REPUBLIC PI W LAFAYETTE PA PURDUE UNIV, 1358 UNIV HALL, W LAFAYETTE, IN 47907-1358 USA SN 0275-1275 J9 J EARLY REPUBL JI J. Early Repub. PD SPR PY 2006 VL 26 IS 1 BP 162 EP 164 DI 10.1353/jer.2006.0013 PG 3 WC History SC History GA 047QA UT WOS:000237892600022 ER PT J AU Bohlman, S O'Brien, S AF Bohlman, S O'Brien, S TI Allometry, adult stature and regeneration requirement of 65 tree species on Barro Colorado Island, Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE allometry; forest structure; functional groups; Panama; tree architecture ID RAIN-FOREST TREES; TROPICAL FORESTS; RESOURCE HETEROGENEITY; LIGHT TRANSMITTANCE; NEOTROPICAL FOREST; SHADE TOLERANCE; FRENCH-GUIANA; LIFE-HISTORY; CANOPY GAPS; CENSUS PLOT AB This study provides a community-level analysis of how regeneration requirement and adult stature are related to tree allometry (diameter, height and crown size) throughout post-seedling ontogeny on Barro Colorado Island, Panama. Comparing 65 species, gap species are taller, have higher diameter growth rates and occupy more low-canopy sites (<= 10 m canopy height) than shade species at small diameters (<= 10 cm dbh). For trees > 10 cm dbh, diameter-height relationships and growth rates no longer differ between gap and shade species. but shade species have larger, particularly deeper, crowns than gap species. Species with tall adult stature have more slender stems with larger crowns compared with treelet and mid-canopy species starting at 5 cm dbh. From 10 to 40 cm dbh, diameter growth rate is also significantly greater for tall species. The consistent allometric differences between functional groups on a community level will, in part, determine vertical and horizontal stand structure. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Univ Virginia, Sorensen Inst, Charlottesville, VA 22904 USA. RP Bohlman, S (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM sbohlman@princeton.edu NR 63 TC 49 Z9 49 U1 0 U2 20 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2006 VL 22 BP 123 EP 136 DI 10.1017/S0266467405003019 PN 2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 013OC UT WOS:000235417600002 ER PT J AU Neff, H Blomster, J Glascock, MD Bishop, RL Blackman, MJ Coe, MD Cowgill, GL Diehl, RA Houston, S Joyce, AA Lipo, CP Stark, BL Winter, M AF Neff, H Blomster, J Glascock, MD Bishop, RL Blackman, MJ Coe, MD Cowgill, GL Diehl, RA Houston, S Joyce, AA Lipo, CP Stark, BL Winter, M TI Methodological issues in the provenance investigation of Early Formative Mesoamerican ceramics SO LATIN AMERICAN ANTIQUITY LA English DT Article ID NEUTRON-ACTIVATION ANALYSIS; ARCHAEOLOGICAL CERAMICS; MOTHER CULTURE; POTTERY; MEXICO; OLMEC; PERSPECTIVE AB A recent study of Early Formative Mesoamerican pottery by instrumental neutron activation analysis (INAA) yielded surprising results that prompted two critiques in the Proceedings of the National Academy of Sciences. The INAA study indicated that the Olmec center of San Lorenzo was a major exporter of carved-incised and white pottery and that little if any pottery made elsewhere was consumed at San Lorenzo. The critiques purport to '' overturn '' the INAA study and demonstrate a more balanced exchange of pottery among Early Formative centers. However, the critiques rely on a series of mistaken claims and misunderstandings that are addressed here. New petrographic data on a small sample of Early Formative pottery (Stoltman et al. 2005) are potentially useful, but they do not overturn INAA of nearly 1000 pottery samples and hundreds of raw material samples. C1 Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA. Calif State Univ Long Beach, Inst Integrated Res Mat Environm & Soc, Long Beach, CA 90840 USA. George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20013 USA. Yale Univ, Peabody Museum, Dept Anthropol, New Haven, CT 06520 USA. Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. Univ Alabama, Dept Anthropol, Tuscaloosa, AL 35487 USA. Brown Univ, Dept Anthropol, Providence, RI 02912 USA. Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. Ctr INAH Oaxaca, Oaxaca 68000, Mexico. RP Neff, H (reprint author), Calif State Univ Long Beach, Dept Anthropol, 1250 Bellflower Blvd, Long Beach, CA 90840 USA. OI Glascock, Michael D./0000-0003-0686-7556 NR 64 TC 40 Z9 40 U1 4 U2 12 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD MAR PY 2006 VL 17 IS 1 BP 54 EP 76 PG 23 WC Archaeology SC Archaeology GA 030KL UT WOS:000236633300003 ER PT J AU Ubelaker, DH Stothert, KE AF Ubelaker, DH Stothert, KE TI Elemental analysis of alkalis and dental deposits associated with coca chewing in Ecuador SO LATIN AMERICAN ANTIQUITY LA English DT Article ID CALCULUS; SUPRAGINGIVAL; SUBGINGIVAL; PERU AB The relationship between Andean coca use and dental deposits is explored through the use of scanning electron microscopy/energy dispersive X-ray, spectroscopy, (SEM/EDS). Elemental analyses of samples of large dental deposits from archeologically recovered skeletons from Ecuador dating between 500 B. C and A.D. 1532 are compared with those of nominal calculus deposits of individuals from North America (modern and precontact), of normal tooth structure and of samples of alkali recovered from Ecuadorian artifacts thought to have been employed in coca use. Spectral analysis revealed homogeneity among all dental samples (deposits and structure) and that they are distinct from the elemental pattern revealed in the analysis of the artifact alkalis. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. Univ Texas, Ctr Archaeol Res, San Antonio, TX 78249 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. EM ubelaked@si.edu NR 39 TC 1 Z9 1 U1 2 U2 5 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD MAR PY 2006 VL 17 IS 1 BP 77 EP 89 PG 13 WC Archaeology SC Archaeology GA 030KL UT WOS:000236633300004 ER PT J AU Neff, H Blomster, J Glascock, MD Bishop, RL Blackman, MJ Coe, MD Cowgill, GL Cyphers, A Diehl, RA Houston, S Joyce, AA Lipo, CP Winter, M AF Neff, H Blomster, J Glascock, MD Bishop, RL Blackman, MJ Coe, MD Cowgill, GL Cyphers, A Diehl, RA Houston, S Joyce, AA Lipo, CP Winter, M TI Smokescreens in the provenance investigation of Early Formative Mesoamerican ceramics SO LATIN AMERICAN ANTIQUITY LA English DT Editorial Material ID ACID-EXTRACTION; COMPOSITIONAL CHARACTERIZATION; ARCHAEOLOGICAL CERAMICS; TEHUACAN PROJECT; ANCIENT MEXICO; MOTHER CULTURE; POTTERY; OLMEC; OAXACA AB We are glad that Sharer et al. (this issue) have dropped their original claim that the INAA data demonstrate multidirectional movement of Early Formative pottery. Beyond this, however, they offer nothing that might enhance understanding of Early Formative ceramic circulation or inspire new insights into Early Formative cultural evolution in Mesoamerica. Instead, their response contains fresh distortions, replications of mistakes made in their PNAS articles, and lengthy passages that are irrelevant to the issues raised by Neff et al. (this issue). We correct and recorrect their latest distortions and misunderstandings here. Besides showing why their discussion of ceramic sourcing repeatedly misses the mark, we also correct a number of erroneous assertions about the archaeology of Olmec San Lorenzo. New evidence deepens understanding of Early Formative Mesoamerica but requires that some researchers discard cherished beliefs. C1 Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA. Calif State Univ Long Beach, Inst Integrated Res Mat Environm & Soc, Long Beach, CA 90840 USA. George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20013 USA. Yale Univ, Peabody Museum, Dept Anthropol, New Haven, CT 06520 USA. Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. Univ Nacl Autonoma Mexico, Inst Invest Antropol, Mexico City 04510, DF, Mexico. Univ Alabama, Dept Anthropol, Tuscaloosa, AL 35487 USA. Brown Univ, Dept Anthropol, Providence, RI 02912 USA. Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. Ctr INAH Oaxaca, Oaxaca 68000, Mexico. RP Neff, H (reprint author), Calif State Univ Long Beach, Dept Anthropol, 1250 Bellflower Blvd, Long Beach, CA 90840 USA. OI Glascock, Michael D./0000-0003-0686-7556 NR 53 TC 29 Z9 29 U1 0 U2 3 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD MAR PY 2006 VL 17 IS 1 BP 104 EP 118 PG 15 WC Archaeology SC Archaeology GA 030KL UT WOS:000236633300006 ER PT J AU Torres, EP Foley, DH Bryan, JH AF Torres, EP Foley, DH Bryan, JH TI Molecular systematics of the Philippine malaria vector Anopheles flavirostris SO MEDICAL AND VETERINARY ENTOMOLOGY LA English DT Article DE Anopheles flavirostris; allozymes; cytochrome c oxidase subunit I; internal transcribed spacer 2; malaria; mitochondrial DNA; phylogenetics; systematics; third domain; Philippines ID SUBGENUS CELLIA DIPTERA; PHYLOGENETIC-RELATIONSHIPS; MINIMUS GROUPS; CULICIDAE; COMPLEX; MEMBERS; IDENTIFICATION; POLYMORPHISM; SEQUENCES; MOSQUITOS AB Allozyme and molecular sequence data from the malaria vector Anopheles flavirostris (Ludlow) (Diptera: Culicidae) were analysed from 34 sites throughout the Philippines, including the type locality, to test the hypothesis that this taxon is a single panmictic species. A finer-scaled allozyme study, of mainly Luzon samples, revealed no fixed genetic differences in sympatric sites and only low levels of variation. We obtained data from partial sequences for the internal transcribed spacer 2 (ITS2) (483 bp), the third domain (D3) (330 bp) of the 28S ribosomal DNA subunit and cytochrome c oxidase subunit I (COI) of mitochondrial DNA (261 bp). No sequence variation was observed for ITS2, only a one base pair difference was observed between Philippine and Indonesian D3 sequences and An. flavirostris sequences were unique, confirming their diagnostic value for this taxon. Sixteen COI haplotypes were identified, giving 25 parsimony informative sites. Neighbour-Joining, Maximum Parsimony, Maximum Likelihood and Bayesian phylogenetic analysis of COI sequences for An. flavirostris and outgroup taxa revealed strong branch support for the monophyly of An. flavirostris, thus confirming that Philippine populations of this taxon comprise a single separate species within the Minimus Subgroup of the Funestus Group. Variation in the behaviour of An. flavirostris is likely to be intraspecific rather than interspecific in origin. C1 Res Inst Trop Med, Manila, Philippines. Queensland Inst Med Res, Brisbane, Qld 4006, Australia. Univ Queensland, Trop Hlth Program, Australian Ctr Int & Trop Hlth & Nutr, Brisbane, Qld, Australia. RP Foley, DH (reprint author), Smithsonian Inst, WRBU, MSC MRC534, Suitland, MD 20746 USA. EM foleydes@si.edu OI Foley, Desmond/0000-0001-7525-4601 FU Wellcome Trust NR 37 TC 5 Z9 7 U1 2 U2 4 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0269-283X J9 MED VET ENTOMOL JI Med. Vet. Entomol. PD MAR PY 2006 VL 20 IS 1 BP 44 EP 52 DI 10.1111/j.1365-2915.2006.00610.x PG 9 WC Entomology; Veterinary Sciences SC Entomology; Veterinary Sciences GA 024DH UT WOS:000236174700005 PM 16608489 ER PT J AU Jones, FA Hamrick, JL Peterson, CJ Squiers, ER AF Jones, FA Hamrick, JL Peterson, CJ Squiers, ER TI Inferring colonization history from analyses of spatial genetic structure within populations of Pinus strobus and Quercus rubra SO MOLECULAR ECOLOGY LA English DT Article DE allozymes; colonization; kinship; mating system; seed dispersal; spatial autocorrelation ID NORTHERN RED OAK; WHITE-PINE; SEED DISPERSAL; AUTOCORRELATION ANALYSIS; ALLOZYME POLYMORPHISMS; TURKEY OAK; TREE; FOREST; SEEDLINGS; REGENERATION AB Many factors interact to determine genetic structure within populations including adult density, the mating system, colonization history, natural selection, and the mechanism and spatial patterns of gene dispersal. We examined spatial genetic structure within colonizing populations of Quercus rubra seedlings and Pintis strobus juveniles and adults in an aspen-white pine forest in northern Michigan, USA. A 20-year spatially explicit demographic study of the forest enables us to interpret the results in light of recent colonization of the site for both species. We assayed 217 Q. rubra seedlings and 171 P. strobus individuals at 11 polymorphic loci using nine allozyme systems. Plant genotypes and locations were used in an analysis of spatial genetic structure. Q. rubra and A strobus showed similar observed levels of heterozygosity, but Q. rubra seedlings have less heterozygosity than expected. Q. rubra seedlings show spatial genetic clumping of individuals on a scale to 25 m and levels of genetic relatedness expected from the clumped dispersion of half-siblings. In contrast, P. strobus has low levels of genetic relatedness at the smallest distance class and positive spatial genetic structure at scales < 10 m within the plot. The low density of adult Q. rubra outside the study plot and limited, spatially clumped rodent dispersal of acorns is likely responsible for the observed pattern of spatial genetic structure and the observed heterozygote deficit (i.e. a Wahlund effect). We attribute weaker patterns observed in P. strobus to the longer dispersal distance of seeds and the historical overlap of seed shadows from adults outside of the plot coupled with the overlap of seed shadows from younger, more recently established reproductive adults. The study demonstrates the utility of long-term demographic data in interpreting mechanisms responsible for generating contemporary patterns of genetic structure within populations. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Univ Georgia, Dept Genet, Athens, GA 30602 USA. Taylor Univ, Dept Earth & Environm Sci, Upland, IN 46989 USA. RP Jones, FA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM jonesf@si.edu RI Jones, Andy/C-3460-2009 NR 74 TC 39 Z9 41 U1 2 U2 22 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD MAR PY 2006 VL 15 IS 3 BP 851 EP 861 DI 10.1111/j.1365-294X.2005.02830.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 024ON UT WOS:000236205600022 PM 16499707 ER PT J AU Burgess, SL Fleischer, RC AF Burgess, SL Fleischer, RC TI Isolation and characterization of polymorphic microsatellite loci in the Hawaiian flycatcher, the elepaio (Chasiempis sandwichensis) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Chasiempis; elepaio; Hawaii; primers; microsatellites AB Thirteen polymorphic microsatellite loci were isolated and characterized from two clades of an endemic Hawaiian flycatcher, the elepaio (Chasiempis sandwichensis). Seven dinucleotide repeats and one trinucleotide repeat were cloned from Kauai elepaio; five dinucleotide repeats were cloned from Oahu elepaio. Polymorphism was assessed in a sample of Oahu elepaio (n = 22) revealing two to 16 alleles per locus. Observed heterozygosity ranged from 0.14 to 0.91. However, linkage analysis exposed highly significant linkage disequilibrium between two of the most polymorphic loci. Twelve loci are therefore expected to be useful for investigations of population structure. C1 Univ Hawaii, John A Burns Sch Med, Dept Cell & Mol Biol, Evolut Ecol & Conservat Biol Program, Honolulu, HI 96822 USA. Smithsonian Inst, Museum Natl Hist Nat, Genet Program, Washington, DC 20008 USA. RP Burgess, SL (reprint author), Univ Hawaii, John A Burns Sch Med, Dept Cell & Mol Biol, Evolut Ecol & Conservat Biol Program, 1960 East West Rd, Honolulu, HI 96822 USA. EM slb@hawaii.edu NR 8 TC 3 Z9 3 U1 0 U2 5 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD MAR PY 2006 VL 6 IS 1 BP 14 EP 16 DI 10.1111/j.1471-8286.2005.01093.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 017XC UT WOS:000235725600005 ER PT J AU Mavarez, J Gonzalez, M AF Mavarez, J Gonzalez, M TI A set of microsatellite markers for Heliconius melpomene and closely related species SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Heliconius; Lepidoptera; microsatellites; Nymphalidae ID BUTTERFLIES; MIMICRY AB The butterflies in the genus Heliconius offer an exceptional opportunity for the study of the ecology and genetics of an adaptive radiation due to their extensive intra- and interspecific variation in wing colour patterns and mimetic associations. Here, we characterize 22 polymorphic microsatellite loci in Heliconius melpomene that have been shown to be useful for linkage mapping and population studies in this and other species. Levels of variation were high, although heterozygosity deficiencies were found in most loci, probably due to null alleles. The loci showed broad amplification success on six other species across the genus. C1 Smithsonian Trop Res Inst, Ancon, Panama. RP Mavarez, J (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Ancon, Panama. EM mavarezj@si.edu NR 8 TC 13 Z9 13 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD MAR PY 2006 VL 6 IS 1 BP 20 EP 23 DI 10.1111/j.1471-8286.2005.01115.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 017XC UT WOS:000235725600007 ER PT J AU Night, C Nagamine, K Springel, V Hernquist, L AF Night, C Nagamine, K Springel, V Hernquist, L TI Lyman break galaxies at z=4-6 in cosmological smoothed particle hydrodynamics simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : evolution; galaxies : formation; cosmology : theory ID HIGH-REDSHIFT GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; STAR-FORMING GALAXIES; DARK-MATTER; PHOTOMETRIC PROPERTIES; RADIATIVE-TRANSFER; ALPHA ABSORBERS; CLUMPY UNIVERSE; BLACK-HOLES; DEEP SURVEY AB We perform a spectrophotometric analysis of galaxies at redshifts z = 4-6 in cosmological smoothed particle hydrodynamics simulations of a Lambda cold dark matter universe. Our models include radiative cooling and heating by a uniform ultraviolet (UV) background, star formation, supernova feedback, and a phenomenological model for galactic winds. Analysing a series of simulations of varying box size and particle number allows us to isolate the impact of numerical resolution on our results. Specifically, we determine the luminosity functions in B, V, R, i' and z' filters, and compare the results with observational surveys of Lyman break galaxies (LBGs) performed with the Subaru telescope and the Hubble Space Telescope. We find that the simulated galaxies have UV colours consistent with observations and fall in the expected region of the colour-colour diagrams used by the Subaru group. The stellar masses of the most massive galaxies in our largest simulation increase their stellar mass from M-star similar to 10(11) M-circle dot at z = 6 to M-star similar to 10(11.7) M(circle dot)at z= 3. Assuming a uniform extinction of E(B-V) = 0.15, we also find reasonable agreement between simulations and observations in the space density of UV bright galaxies at z = 3-6, down to the magnitude limit of each survey. For the same moderate extinction level of E(B-V) similar to 0.15, the simulated luminosity functions match observational data, but have a steep faint-end slope with alpha similar to -2.0. We discuss the implications of the steep faint-end slope found in the simulations. Our results confirm the generic conclusion from earlier numerical studies that UV bright LBGs at z >= 3 are the most massive galaxies with E(B-V) similar to 0.15 at each epoch. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Night, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cnight@cfa.harvard.edu; knagamine@ucsd.edu; volker@mpa-garching.mpg.de; lars@cfa.harvard.edu NR 52 TC 41 Z9 41 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2006 VL 366 IS 3 BP 705 EP 716 DI 10.1111/j.1365-2966.2005.09730.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012IW UT WOS:000235333100001 ER PT J AU Gulati, A AF Gulati, A TI An ounce of prevention ... (Fire prevention in museums) SO MUSEUM NEWS LA English DT Editorial Material C1 Smithsonian Inst, Off Safety Hlth & Environm Management, Washington, DC 20560 USA. RP Gulati, A (reprint author), Smithsonian Inst, Off Safety Hlth & Environm Management, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2006 VL 85 IS 2 BP 11 EP 12 PG 2 WC Art SC Art GA 044ZQ UT WOS:000237712800003 ER PT J AU Norwood, J AF Norwood, J TI Caring for American Indian objects: A practical and cultural guide. SO MUSEUM NEWS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Museum Training Program, Washington, DC 20560 USA. RP Norwood, J (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Museum Training Program, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2006 VL 85 IS 2 BP 25 EP 26 PG 2 WC Art SC Art GA 044ZQ UT WOS:000237712800009 ER PT J AU McQuinn, M Furlanetto, SR Hernquist, L Zahn, O Zaldarriaga, M AF McQuinn, M Furlanetto, SR Hernquist, L Zahn, O Zaldarriaga, M TI The kinetic Sunyaev-Zel'dovich effect from reionization SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT First Light and Reionization - Theoretical Study and Experimental Detection of First Luminous Sources in the Universe CY MAY 18-21, 2005 CL Irvine, CA DE cosmology : theory; intergalactic medium; cosmic microwave background ID MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; COSMIC REIONIZATION; STELLAR SOURCES; POLARIZATION; IONIZATION; GALAXIES; STARS; TEMPERATURE AB During the epoch of reionization, local variations in the ionized fraction (patchiness) imprint arcminute-scale temperature anisotropies in the cosmic microwave background through the kinetic Sunyaev-Zel'dovich (kSZ) effect. We employ an analytic model of reionization devised by Furlanetto and coworkers to calculate the kSZ anisotropies for patchy reionization. We find that the angular power spectrum of the kSZ anisotropies depends strongly on the size distribution of the HII bubbles and on the duration of reionization. In addition, we show that upcoming measurements of the kSZ effect should be able to distinguish between several popular reionization scenarios. In particular, the amplitude of the patchy power spectrum for reionization scenarios in which the IGM is significantly ionized by Population III stars (or by mini-quasars/decaying particles) can be larger (or smaller) by over a factor of 3 than the amplitude in more traditional reionization histories (with temperature anisotropies that range between 0.5 and 3 mu K at l = 5000). (c) 2005 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP McQuinn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmcquinn@cfa.harvard.edu NR 27 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 EI 1872-9630 J9 NEW ASTRON REV JI New Astron. Rev. PD MAR PY 2006 VL 50 IS 1-3 BP 84 EP 88 DI 10.1016/j.newar.2005.11.025 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018ET UT WOS:000235747500014 ER PT J AU Windhorst, RA Cameron, RA Brissenden, RJ Elvis, MS Fabbiano, G Gorenstein, P Reid, PB Schwartz, DA Bautz, MW Figueroa-Feliciano, E Petre, R White, NE Zhang, WW AF Windhorst, RA Cameron, RA Brissenden, RJ Elvis, MS Fabbiano, G Gorenstein, P Reid, PB Schwartz, DA Bautz, MW Figueroa-Feliciano, E Petre, R White, NE Zhang, WW TI Generation-X: An X-ray observatory designed to observe first light objects SO NEW ASTRONOMY REVIEWS LA English DT Article; Proceedings Paper CT First Light and Reionization - Theoretical Study and Experimental Detection of First Luminous Sources in the Universe CY MAY 18-21, 2005 CL Irvine, CA DE Gen-X; vision mission; X-ray astronomy; active optics; lightweight optics ID STAR-FORMATION RATE; FIELD NORTH SURVEY; SOURCE CATALOGS; BLACK-HOLES; GALAXIES; BINARIES AB The new cosmological frontier will be the study of the very first stars, galaxies and black holes in the early Universe. These objects are invisible to the current generation of X-ray telescopes, such as Chandra. In response, the Generation-X ('' Gen-X '') Vision Mission has been proposed as a future X-ray observatory which will be capable of detecting the earliest objects. X-ray imaging and spectroscopy of such faint objects demands a large collecting area and high angular resolution. The Gen-X mission plans 100 m(2) collecting area at 1 keV (1000x that of Chandra), and with an angular resolution of 0.1 ''. The Gen-X mission will operate at Sun-Earth L2, and might involve four 8 m diameter telescopes or even a single 20 m diameter telescope. To achieve the required effective area with reasonable mass, very lightweight grazing incidence X-ray optics must be developed, having an areal density 100x lower than in Chandra, with mirrors as thin as 0.1 mm requiring active on-orbit figure control. The suite of available detectors for Gen-X should include a large-area high resolution imager, a cryogenic imaging spectrometer, and a grating spectrometer. We discuss use of Gen-X to observe the birth of the first black holes, stars and galaxies, and trace their cosmic evolution. (c) 2005 Elsevier B.V. All rights reserved. C1 Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Windhorst, RA (reprint author), Arizona State Univ, Dept Phys & Astron, Box 871504, Tempe, AZ 85287 USA. EM Rogier.Windhorst@asu.edu RI White, Nicholas/B-6428-2012 OI White, Nicholas/0000-0003-3853-3462 NR 22 TC 20 Z9 20 U1 2 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD MAR PY 2006 VL 50 IS 1-3 BP 121 EP 126 DI 10.1016/j.newar.2005.11.019 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018ET UT WOS:000235747500020 ER PT J AU Novikova, I Phillips, DF Zibrov, AS Walsworth, RL Taichenachev, AV Yudin, VI AF Novikova, I Phillips, DF Zibrov, AS Walsworth, RL Taichenachev, AV Yudin, VI TI Cancellation of light shifts in an N-resonance clock SO OPTICS LETTERS LA English DT Article AB We demonstrate that first-order light shifts can be canceled for an all-optical, three-photon-absorption resonance (N-resonance) on the D, transition of Rb-87. This light-shift cancellation facilitates improved frequency stability for an N-resonance clock. For example, by using a tabletop apparatus designed for N-resonance spectroscopy, we measured a short-term fractional frequency stability (Allan deviation) of similar or equal to 1.5 x 10(-11) (tau)-1/2 for observation times of 1 s <= tau <= 50 s. Further improvements in frequency stability should be possible with an apparatus designed as a dedicated N-resonance clock. (c) 2006 Optical Society of America. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Novosibirsk State Univ, Novosibirsk 630090, Russia. RAS, SB, Inst Laser Phys, Novosibirsk 630090, Russia. RP Novikova, I (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM i.novikova@osa.org RI Novikova, Irina/B-9041-2008; Taichenachev, Aleksei/K-7065-2015; Zibrov, Alexander/G-7419-2014 OI Taichenachev, Aleksei/0000-0003-2273-0066; NR 8 TC 18 Z9 18 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD MAR 1 PY 2006 VL 31 IS 5 BP 622 EP 624 DI 10.1364/OL.31.000622 PG 3 WC Optics SC Optics GA 015DR UT WOS:000235532600020 PM 16570418 ER PT J AU Calderon, AI Vazquez, Y Solis, PN Caballero-George, C Zacchino, S Gimenez, A Pinzon, R Caceres, A Tamayo, G Correa, M Gupta, MP AF Calderon, AI Vazquez, Y Solis, PN Caballero-George, C Zacchino, S Gimenez, A Pinzon, R Caceres, A Tamayo, G Correa, M Gupta, MP TI Screening of Latin American plants for cytotoxic activity SO PHARMACEUTICAL BIOLOGY LA English DT Article DE Blepharocalyx salicifolius; cytotoxicity; Latin American biodiversity; Piper barbatum; Senna occidentalis; SRB assay; Thevetia ahouai ID ANTICANCER DRUG SCREEN; ANNONA-MURICATA; ENTEROLOBIUM-CONTORTISILIQUUM; TRITERPENE BISDESMOSIDES; PIPER-SINTENENSE; HELA-CELLS; ACETOGENINS; CONSTITUENTS; PHYSALINS; LEAVES AB The SRB cytotoxicity assay was used to screen plant extracts, in a collaborative multinational OAS project involving Argentina, Bolivia, Colombia, Costa Rica, Guatemala, Nicaragua and Panama, against breast (MCF-7), lung (H-460), and central nervous system (SF-268) human cancer cell lines. Out of 310 species tested, 23 (7.4%) plants showed cytotoxic activity at GI 50 values <= 10 mu g/ml. The most active plants were Thevetia ahouai , Physalis viscosa , Piper jacquemontianum , Piper barbatum , Senna occidentalis , Tovomita longifolia , and Lippia cardiostegia . Blepharocalyx salicifolius and Senna occidentalis were selectively active against one cell line, SF-268 or MCF-7, respectively. Within the framework of this project, 14 compounds have been isolated, 5 new (4 benzophenones, coumarin) and 9 known to the literature. But only the bioassay-guided fractionation of the active extract of Piper barbatum leaves, which led to the isolation of three known compounds: (2' E , 6' E )-2-farnesyl-1,4-benzoquinone (1), (2' E , 6' E )-2-farnesylhydroquinone (2), and dictyochromenol (3), is reported here. The chemical structures of 1 and 2 were determined by spectral means (1D, 2D NMR, MS) and chemical data. Among these three, (2' E , 6' E )-2-farnesyl-1,4-benzoquinone was the most active (MCF-7 GI(50) = 1.8 mu g/ml; H-460 GI(50) = 4.8 mu g/ml; SF-268 GI(50) = 3.5 mu g/ml). C1 Univ Panama, CIFLORPAN, Fac Farm, Panama City, Panama. Univ Nacl Rosario, Fac Ciencias Bioquim & Farmaceut, Rosario, Argentina. Univ Mayor San Andres, Inst Invest Farmaco Bioquim, La Paz, Bolivia. Univ Nacl Colombia, Dept Farm, Bogota, Colombia. Univ San Carlos, Fac Ciencias Quim & Farm, Guatemala City, Guatemala. Inst Nacl Biodiversidad INBIO, San Jose, Costa Rica. Univ Costa Rica, Ezcuela Quim, San Jose, Costa Rica. Smithsonian Trop Res Inst, Panama City, Panama. RP Gupta, MP (reprint author), Univ Panama, CIFLORPAN, Fac Farm, Panama City, Panama. EM cytedqff@ancon.up.ac.pa RI Tamayo, Giselle/J-3609-2015; OI Tamayo, Giselle/0000-0002-4912-8895; Gupta, Mahabir/0000-0002-9302-7864 NR 36 TC 10 Z9 14 U1 2 U2 21 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 MAR PY 2006 VL 44 IS 2 BP 130 EP 140 DI 10.1080/13880200600592285 PG 11 WC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy SC Plant Sciences; Medical Laboratory Technology; Pharmacology & Pharmacy GA 021UM UT WOS:000236011400011 ER PT J AU Fischer, JM Fields, PA Pryzbylkowski, PG Nicolai, JL Neale, PJ AF Fischer, JM Fields, PA Pryzbylkowski, PG Nicolai, JL Neale, PJ TI Sublethal exposure to UV radiation affects respiration rates of the freshwater cladoceran Daphnia catawba SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID INDUCED DNA-DAMAGE; ULTRAVIOLET-RADIATION; REPAIR; TEMPERATURE; ZOOPLANKTON; DEPTH AB We examined the effects of UV radiation (UVR) on metabolic rates of the freshwater cladoceran Daphyda catawba. We exposed D. catawba to UVB for 12 h in a lamp phototron at levels of 2.08 and 4.16 kJ m(-2) both with and without concomitant exposure to UVA and visible photorepair radiation (PRR). We also included a group that received PRR only and a dark control group. Respiration rates were measured for 6 h following exposure. Respiration rates increased by 31.8% relative to the dark control at the lowest level of UVB stress (2.08 kJ m(-2) UVB with PRR), whereas respiration was inhibited by 70.3% at the highest stress level (4.16 kJ m(-2) UVB without PRR). Survival rates in the group that received PRR only and the group exposed to 2.08 kJ m(-2) and PRR were not significantly different from that in the control group; however, the survival rate was reduced for all other UVR exposures. We hypothesize that enhanced respiration rates reflect energetic costs related to repair of cellular components damaged by sublethal levels of UVR. Increases in respiration rate of the magnitude we found in our experiment could significantly reduce energetic reserves available for growth and reproduction, especially in cases where these costs are incurred repeatedly during a series of days with high levels of UVR. C1 Franklin & Marshall Coll, Dept Biol, Lancaster, PA 17604 USA. Smithsonian Environm Res Ctr, Edgewater, MD USA. RP Fischer, JM (reprint author), Franklin & Marshall Coll, Dept Biol, Lancaster, PA 17604 USA. EM jfischer@fandm.edu RI Neale, Patrick/A-3683-2012 NR 20 TC 28 Z9 30 U1 1 U2 12 PU AMER SOC PHOTOBIOLOGY PI AUGUSTA PA BIOTECH PARK, 1021 15TH ST, SUITE 9, AUGUSTA, GA 30901-3158 USA SN 0031-8655 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD MAR-APR PY 2006 VL 82 IS 2 BP 547 EP 550 DI 10.1562/2005-08-30-RA-664 PG 4 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 036CK UT WOS:000237048300030 PM 16613511 ER PT J AU Daw, A Gardner, LD Janzen, PH Kohl, JL AF Daw, A Gardner, LD Janzen, PH Kohl, JL TI Absolute cross section for C2+(2s2p P-3(o)-> 2p(2) P-3) electron-impact excitation SO PHYSICAL REVIEW A LA English DT Article ID ION EXCITATION; C-III; ULTRAVIOLET-SPECTRUM; BEAMS; C2+; CAPTURE; STATES; FUSE; SUN AB We have measured the absolute energy-averaged cross section for the electron impact excitation of C2+(2s2p P-3(o)-> 2p(2) P-3) from energies below threshold to 17 eV above, and present the measured absolute rate coefficients for this transition, for temperatures from 10(4) to 10(5) K. These rate coefficients are required for diagnostics of plasmas such as those found in astrophysical environments. The synchronous photon detection method with beams modulation and inclined electron and ion beams was used. Radiation at 117.6 nm from the decay of the excited ions back to the metastable state was detected using an absolutely calibrated optical system. The fractional population of metastable C2+(2s2p P-3(o)) in the incident ion beam was determined to be 0.42 +/- 0.03(1.65 sigma). The rate coefficient for log(10) T=4.8 was determined to be 1.01x10(-8) cm(3) s(-1)+/- 14% at a 90% confidence (1.65 sigma) level. The measured cross section is in agreement within experimental uncertainty with 6-term close-coupling R-matrix calculations and 90-term R matrix with pseudostates calculations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Daw, A (reprint author), Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. RI daw, adrian/D-2297-2012 NR 25 TC 3 Z9 3 U1 1 U2 2 PU AMERICAN 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 MAR PY 2006 VL 73 IS 3 AR 032709 DI 10.1103/PhysRevA.73.032709 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 028DQ UT WOS:000236467500095 ER PT J AU Dutta, CM Oubre, C Nordlander, P Kimura, M Dalgarno, A AF Dutta, CM Oubre, C Nordlander, P Kimura, M Dalgarno, A TI Charge-transfer cross sections in collisions of ground-state Ca and H+ SO PHYSICAL REVIEW A LA English DT Article ID SODIUM-D-LINES; ATOMIC-HYDROGEN; SHIFT AB We have investigated collisions of Ca(4s(2)) with H+ in the energy range of 200 eV/u-10 keV/u using the semiclassical molecular-orbital close-coupling (MOCC) method with 18 coupled molecular states (11 (1)Sigma(+) and seven (1)Pi(+) states) to determine charge-transfer cross sections. Except for the incoming channel 6 (1)Sigma(+), the molecular states all correspond to charge-transfer channels. Inclusion of Ca2+-H- is crucial in the configuration-interaction calculation for generating the molecular wave functions and potentials. Because of the Coulomb attraction, the state separating to Ca2+-H- creates many avoided crossings, even though at infinite separation it lies energetically above all other states that we included. Because of the avoided crossings between the incoming channel 6 (1)Sigma(+) and the energetically close charge-transfer channel 7 (1)Sigma(+) the charge-transfer interaction occurs at long range. This makes calculations of charge-transfer cross sections by the MOCC method very challenging. The total charge-transfer cross sections increase monotonically from 3.4x10(-15) cm(2) at 200 eV/u to 4.5x10(-15) cm(2) at 10 keV/u. Charge transfer occurs mostly to the excited Ca+(5p) state in the entire energy range, which is the sum of the charge transfer to 7 (1)Sigma(+) and 4 (1)Pi(+). It accounts for similar to 47% of the total charge transfer cross sections at 200 eV/u. However, as the energy increases, transfer to Ca+(4d) increases, and at 10 keV/u the charge-transfer cross sections for Ca+(5p) and Ca+(4d) become comparable, each giving similar to 38% of the total cross section. C1 Rice Univ, Dept Phys, Houston, TX 77251 USA. Rice Univ, Rice Quantum Inst, Houston, TX 77251 USA. Kyushu Univ, Grad Sch Sci, Fukuoka 8128581, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dutta, CM (reprint author), Rice Univ, Dept Phys, Houston, TX 77251 USA. RI Nordlander, Peter/A-2560-2008 OI Nordlander, Peter/0000-0002-1633-2937 NR 19 TC 0 Z9 0 U1 0 U2 2 PU AMERICAN 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 MAR PY 2006 VL 73 IS 3 AR 032714 DI 10.1103/PhysRevA.73.032714 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 028DQ UT WOS:000236467500100 ER PT J AU Garofalo, EM AF Garofalo, EM TI Human cranial suture and vault development SO SCANNING LA English DT Meeting Abstract C1 Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FAMS INC PI MAHWAH PA BOX 832, MAHWAH, NJ 07430-0832 USA SN 0161-0457 J9 SCANNING JI Scanning PD MAR-APR PY 2006 VL 28 IS 2 BP 99 EP 99 PG 1 WC Instruments & Instrumentation; Microscopy SC Instruments & Instrumentation; Microscopy GA 035OZ UT WOS:000237012500055 ER PT J AU Fried, G Grosser, B Mah, C AF Fried, G Grosser, B Mah, C TI Virtual microscopy: A tool for sample documentation and dissemination SO SCANNING LA English DT Meeting Abstract C1 Univ Illinois, Inst Genom Biol, Champaign, IL 61820 USA. Univ Illinois, Beckman Inst Adv Sci & Technol, Champaign, IL 61820 USA. Smithsonian Inst, NMNH, Dept Invertebrate Zool, Washington, DC 20560 USA. RI Mah, Christopher/B-5771-2008 NR 0 TC 0 Z9 0 U1 0 U2 0 PU FAMS INC PI MAHWAH PA BOX 832, MAHWAH, NJ 07430-0832 USA SN 0161-0457 J9 SCANNING JI Scanning PD MAR-APR PY 2006 VL 28 IS 2 BP 100 EP 101 PG 2 WC Instruments & Instrumentation; Microscopy SC Instruments & Instrumentation; Microscopy GA 035OZ UT WOS:000237012500057 ER PT J AU Frohlich, B AF Frohlich, B TI Computed tomography at the Smithsonian Institution: Application and evaluation SO SCANNING LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FAMS INC PI MAHWAH PA BOX 832, MAHWAH, NJ 07430-0832 USA SN 0161-0457 J9 SCANNING JI Scanning PD MAR-APR PY 2006 VL 28 IS 2 BP 100 EP 100 PG 1 WC Instruments & Instrumentation; Microscopy SC Instruments & Instrumentation; Microscopy GA 035OZ UT WOS:000237012500056 ER PT J AU Snyder, R AF Snyder, R TI Kennewick Man: Using CT data in a forensic context SO SCANNING LA English DT Meeting Abstract C1 Smithsonian Inst, NMNH, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU FAMS INC PI MAHWAH PA BOX 832, MAHWAH, NJ 07430-0832 USA SN 0161-0457 J9 SCANNING JI Scanning PD MAR-APR PY 2006 VL 28 IS 2 BP 101 EP 101 PG 1 WC Instruments & Instrumentation; Microscopy SC Instruments & Instrumentation; Microscopy GA 035OZ UT WOS:000237012500058 ER PT J AU Whittaker, SD Duckett, CN AF Whittaker, SD Duckett, CN TI Effects of DNA extraction techniques on morphological analysis of small arthropods SO SCANNING LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FAMS INC PI MAHWAH PA BOX 832, MAHWAH, NJ 07430-0832 USA SN 0161-0457 J9 SCANNING JI Scanning PD MAR-APR PY 2006 VL 28 IS 2 BP 102 EP 102 PG 1 WC Instruments & Instrumentation; Microscopy SC Instruments & Instrumentation; Microscopy GA 035OZ UT WOS:000237012500059 ER PT J AU Small, LM AF Small, LM TI Field trip! SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Small, LM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2006 VL 36 IS 12 BP 14 EP 14 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 015YT UT WOS:000235588300002 ER PT J AU Pick, M Forbes, TG Mann, G Cane, HV Chen, J Ciaravella, A Cremades, H Howard, RA Hudson, HS Klassen, A Klein, KL Lee, MA Linker, JA Maia, D Mikic, Z Raymond, JC Reiner, MJ Simnett, GM Srivastava, N Tripathi, D Vainio, R Vourlidas, A Zhang, J Zurbuchen, TH Sheeley, NR Marque, C AF Pick, M. Forbes, T. G. Mann, G. Cane, H. V. Chen, J. Ciaravella, A. Cremades, H. Howard, R. A. Hudson, H. S. Klassen, A. Klein, K. L. Lee, M. A. Linker, J. A. Maia, D. Mikic, Z. Raymond, J. C. Reiner, M. J. Simnett, G. M. Srivastava, N. Tripathi, D. Vainio, R. Vourlidas, A. Zhang, J. Zurbuchen, T. H. Sheeley, N. R. Marque, C. TI Multi-wavelength observations of CMEs and associated phenomena SO SPACE SCIENCE REVIEWS LA English DT Article ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; IMPULSIVE ELECTRON EVENTS; X-RAY OBSERVATIONS; MAGNETIC-FLUX ROPE; SOLAR-FLARE; SHOCK-WAVE; INTERPLANETARY MEDIUM; LASCO OBSERVATIONS; CURRENT SHEET AB This chapter reviews how our knowledge of CMEs and CME-associated phenomena has been improved, since the launch of the SOHO mission, thanks to multi-wavelength analysis. The combination of data obtained from space-based experiments and ground based instruments allows us to follow the space-time development of an event from the bottom of the corona to large distances in the interplanetary medium. Since CMEs originate in the low solar corona, understanding the physical processes that generate them is strongly dependant on coordinated multi-wavelength observations. CMEs display a large diversity in morphology and kinematic properties, but there is presently no statistical evidence that those properties may serve to group them into different classes. When a CME takes place, the coronal magnetic field undergoes restructuring. Much of the current research is focused on understanding how the corona sustains the stresses that allow the magnetic energy to build up and how, later on, this magnetic energy is released during eruptive flares and CMEs. Multi-wavelength observations have confirmed that reconnection plays a key role during the development of CMEs. Frequently, CMEs display a rather simple shape, exhibiting a well known three-part structure (bright leading edge, dark cavity and bright knot). These types of events have led to the proposal of the ''standard model'' of the development of a CME, a model which predicts the formation of current sheets. A few recent coronal observations provide some evidence for such sheets. Other more complex events correspond to multiple eruptions taking place on a time scale much shorter than the cadence of coronagraph instruments. They are often associated with large-scale dimming and coronal waves. The exact nature of these waves and the physical link between these different manifestations are not yet elucidated. We also discuss what kind of shocks are produced during a flare or a CME. Several questions remain unanswered. What is the nature of the shocks in the corona (blast-wave or piston-driven?) How they are related to Moreton waves seen in H alpha? How they are related to interplanetary shocks? The last section discusses the origin of energetic electrons detected in the corona and in the interplanetary medium. "Complex type III-like events,"which are detected at hectometric wavelengths, high in the corona, and are associated with CMEs, appear to originate from electrons that have been accelerated lower in the corona and not at the bow shock of CMEs. Similarly, impulsive energetic electrons observed in the interplanetary medium are not the exclusive result of electron acceleration at the bow shocks of CMEs; rather they have a coronal origin. C1 Observ Paris, CNRS, LESIA, UMR 8109, Meudon, France. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH USA. Astrophys Inst Potsdam, Potsdam, Germany. NASA GSFC, Lab High Energy Astrophys, Greenbelt, MD USA. USN, Res Lab, Plasma Phys Div, Washington, DC USA. INAF Osserv Astron Palermo, Palermo, Italy. Max Planck Inst Sonnenforsch, Katlenburg Duhm, Germany. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Sci Applicat Int Corp, San Diego, CA USA. Univ Porto, Fac Ciencias, Observ Astron, CICGE, Vila Nova De Gaia, Portugal. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA USA. Catholic Univ Amer, Ctr Solar Phys & Space Weather, Washington, DC USA. NASA Goddard Space Flight Ctr, Greenbelt, MD USA. Univ Birmingham, Sch Phys & Space Res, Birmingham, W Midlands, England. Udaipur Solar Observ, Phys Res Lab, Udaipur, India. Univ Helsinki, Dept Phys Sci, Helsinki, Finland. George Mason Univ, Inst Computat Sci, Ctr Earth Observing & Space Res, Fairfield, VA USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI USA. RP Pick, M (reprint author), Observ Paris, CNRS, LESIA, UMR 8109, Meudon, France. EM monique.pick@obspm.fr RI Vainio, Rami/A-5590-2009; Vourlidas, Angelos/C-8231-2009; Tripathi, Durgesh/D-9390-2012 OI Vainio, Rami/0000-0002-3298-2067; Vourlidas, Angelos/0000-0002-8164-5948; Tripathi, Durgesh/0000-0003-1689-6254 NR 153 TC 31 Z9 31 U1 1 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2006 VL 123 IS 1-3 BP 341 EP 382 DI 10.1007/s11214-006-9021-1 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 109SH UT WOS:000242328400015 ER PT J AU Zeder, MA Emshwiller, E Smith, BD Bradley, DG AF Zeder, MA Emshwiller, E Smith, BD Bradley, DG TI Documenting domestication: the intersection of genetics and archaeology SO TRENDS IN GENETICS LA English DT Review ID BEAN PHASEOLUS-VULGARIS; OCA OXALIS-TUBEROSA; GOATS CAPRA-HIRCUS; TOMATO FRUIT SIZE; CATTLE BOS-TAURUS; OLEA-EUROPAEA L.; WILD RELATIVES; ANCIENT DNA; MOLECULAR EVIDENCE; PHYLOGEOGRAPHIC STRUCTURE AB Domestication, a process of increasing mutual dependence between human societies and the plant and animal populations they target, has long been an area of interest in genetics and archaeology. Geneticists seek out markers of domestication in the genomes of domesticated species, both past and present day. Archaeologists examine the archaeological record for complementary markers - evidence of the human behavior patterns that cause the genetic changes associated with domestication, and the morphological changes in target species that result from them. In this article, we summarize the recent advances in genetics and archaeology in documenting plant and animal domestication, and highlight several promising areas where the complementary perspectives of both disciplines provide reciprocal illumination. C1 Smithsonian Inst, Archaeobiol Program, Natl Museum Nat Hist, Washington, DC 20560 USA. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Univ Dublin Trinity Coll, Smurfit Inst Genet, Dublin 2, Ireland. RP Zeder, MA (reprint author), Smithsonian Inst, Archaeobiol Program, Natl Museum Nat Hist, Washington, DC 20560 USA. EM zederm@si.edu RI Emshwiller, Eve/B-9875-2008; Bradley, Daniel/A-3240-2012; OI Emshwiller, Eve/0000-0001-8206-0725; Bradley, Daniel G/0000-0001-7335-7092 NR 171 TC 167 Z9 180 U1 10 U2 82 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0168-9525 J9 TRENDS GENET JI Trends Genet. PD MAR PY 2006 VL 22 IS 3 BP 139 EP 155 DI 10.1016/j.tig.2006.01.007 PG 17 WC Genetics & Heredity SC Genetics & Heredity GA 029BY UT WOS:000236534100005 PM 16458995 ER PT J AU Beach, T Dunning, N Luzzadder-Beach, S Cook, DE Lohse, J AF Beach, T Dunning, N Luzzadder-Beach, S Cook, DE Lohse, J TI Impacts of the ancient Maya on soils and soil erosion in the central Maya Lowlands SO CATENA LA English DT Article; Proceedings Paper CT Regional Geomaorphology Conference of the International-Association-of-Geomorphologists CY OCT 27-NOV 02, 2003 CL Mexico City, MEXICO SP Int Assoc Geomorphol, Int Geograph Union, Commiss Land Degradat & Desertificat DE soil erosion; paleosols; Maya Lowlands; Maya Civilization; land degradation ID ENVIRONMENTAL-CHANGE; EL-PETEN; GUATEMALA; AGRICULTURE; AMERICA; BELIZE; KARST; DEFORESTATION; CIVILIZATION; CONSERVATION AB Many studies across the central and southern Maya Lowlands of Belize, Guatemala, Honduras, and Mexico have produced records of land degradation, mostly sedimentation and soil erosion, during the ancient Maya period from before 1000 BC to the Maya Collapse of c. AD 900. This paper provides new data from two sites (Blue Creek and Cancuen), synthesizes more than a decade of the authors' research in Guatemala, Belize, and Mexico, and synthesizes other findings from this region. These research projects analyzed more than 100 excavations in upland and depression sites, cored lakes and wetland sediments, and studied sediments in the field and laboratory using radiocarbon dating, a battery of soil chemistry tests, stratigraphic analysis, magnetic susceptibility, elemental analyses, and artifact identification. Our objective was to date when sedimentation and soil erosion occurred, identify stable surfaces, and correlate them with the state of knowledge about past land use. These findings indicate three general epochs of accelerated soil erosion and identified two major paleosols. The three waves of soil erosion occurred in the Preclassic period (c. 1000 BC to AD 250), the Late Classic (AD 550 to 900), and in the last several decades. The major paleosol ('Eklu'um') in these sites is a well-developed Mollisol or Vertisol that started forming in the early Holocene and was buried in either the Preclassic or Classic periods (AD 250 to 900). At some sites the Eklu'um paleosol lies beneath sediments with a fainter palcosol, which in turn lies buried below Classic period and later sediments. This picture shows higher than expected soil erosion linked to the region's first pioneer farmers in the Preclassic and less than expected soil erosion in the Late Classic when population peaked and land use was the most intensive, In other regions like Cancuen, Guatemala, however, most soil erosion occurred during the Maya Late Classic (AD 550-830). Erosion here was intense but short-lived: depressions record 1-3 m of aggradation in two centuries. A third epoch of accelerated soil loss and aggradation arose with the rapid land use changes brought by new pioneers during the last several decades. (c) 2005 Elsevier B.V. All rights reserved. C1 Georgetown Univ, SFS, STIA, Washington, DC 20057 USA. Univ Cincinnati, Dept Geog, Cincinnati, OH 45221 USA. George Mason Univ, Sch Computat Sci, Fairfax, VA 22030 USA. Smithsonian Inst, SCMRE, Suitland, MD 20746 USA. Univ Texas, Texas Archeol Res Lab, Austin, TX 78712 USA. RP Beach, T (reprint author), Georgetown Univ, SFS, STIA, Washington, DC 20057 USA. EM beacht@georgetown.edu OI Cook, Duncan/0000-0001-5270-4569 NR 67 TC 63 Z9 69 U1 4 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0341-8162 J9 CATENA JI Catena PD FEB 28 PY 2006 VL 65 IS 2 BP 166 EP 178 DI 10.1016/j.catena.2005.11.007 PG 13 WC Geosciences, Multidisciplinary; Soil Science; Water Resources SC Geology; Agriculture; Water Resources GA 024AA UT WOS:000236166100007 ER PT J AU Peslier, AH Luhr, JF AF Peslier, AH Luhr, JF TI Hydrogen loss from olivines in mantle xenoliths from Simcoe (USA) and Mexico: Mafic alkalic magma ascent rates and water budget of the sub-continental lithosphere SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE water; olivine; xenolith; hydrogen loss; host-magma ascent rate; continental upper-mantle ID NOMINALLY ANHYDROUS MINERALS; OVERLYING SUBDUCTION ZONES; OXIDATION-STATE; OXYGEN FUGACITY; HIGH-PRESSURE; PLASTIC-DEFORMATION; SILICA ACTIVITY; CREEP REGIME; OH DEFECTS; SOLUBILITY AB Olivines in spinel-peridotite mantle xenoliths from Simcoe (Washington State, USA) and Mexico were analyzed by Fourier-transform infrared spectrometry (FTIR) to determine their water contents. The main OH absorbance peaks of most samples are located between 3600 and 3450 cm(-1) (Group I), with a few samples having minor peaks between 3450 and 3100 cm(-1) (Group II). Olivines from one Mexican sample have larger peaks in Group II than in Group I. Most of these OH peaks are predicted by experimental data from the literature in the appropriate range of silica activities and iron contents. A few high-forsterite olivines, however, have mainly Group I peaks which at these low iron contents is characteristic of low-silica activity. Because these olivines coexist with orthopyroxene in the peridotite, buffering silica activity at relatively high values, their FTIR spectra may reflect disturbance of their hydrogen by melts or fluids, most probably associated with the host magma. In eight out of nine samples for which measurement at the olivine edges was possible, water contents are higher in the grain centers than at their edges, with cross-sections showing typical diffusion profiles. Moreover, water concentrations in some samples increase with olivine size. Loss of hydrogen from the olivine during xenolith transport to the surface is likely responsible for these variations. These water-concentration gradients allowed calculation of the duration of hydrogen loss, which ranges from 18 to 65 h, corresponding to host mafic-alkalic magma ascent rates of 0.2-0.5 m s(-1). The highest measured water contents in olivines from individual xenoliths range from 0 to 6.8 ppm and increase with those of clino- and orthopyroxenes. Differences in hydrogen partition coefficients between olivine and pyroxenes from our data and from experiments suggest that the analyzed olivines lost at least 40% of their water during ascent from the mantle. Olivine water contents do not correlate with partial melting indices, but samples with high olivine water contents generally have low clinopyroxene La/Yb ratios and low spinel Fe(3+)/Sigma Fe ratios and resultant oxygen fugacities, and vice-versa. Metasomatism by fluids or melts and the ambient oxygen fugacity of the mantle may have played roles in the original incorporation of hydrogen into these olivines, but such primary signals have probably been obscured by later hydrogen loss. The systematically lower water contents of olivines in Mexican and Simcoe xenoliths relative to those from cratonic xenoliths may mainly reflect lower host-magma ascent velocities for mafic alkalic magmas compared to kimberlites. Calculated whole-rock water contents for the studied spinel-peridotite xenoliths range from 2.5 to 154 ppm. If 150 ppm, were representative of the water content in the entire upper mantle (to 410 km), the amount of water stored there can be speculated to be only about 0.06 times the equivalent mass of Earth's oceans. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Houston, Texas Ctr Superconduct, Houston, TX 77204 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Peslier, AH (reprint author), Univ Houston, Texas Ctr Superconduct, HSC Bldg 202, Houston, TX 77204 USA. EM apeslier@mail.uh.edu; luhr@volcano.si.edu RI Peslier, Anne/F-3956-2010 NR 68 TC 126 Z9 145 U1 5 U2 26 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 FEB 28 PY 2006 VL 242 IS 3-4 BP 302 EP 319 DI 10.1016/j.epsl.2005.12.019 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 019RT UT WOS:000235855100006 ER PT J AU Lesanovsky, I Schmelcher, P Sadeghpour, HR AF Lesanovsky, I Schmelcher, P Sadeghpour, HR TI Ultra-long-range Rydberg molecules exposed to a magnetic field SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID HYDROGEN-ATOM; H-2 MOLECULE; STATES; POSITRONIUM; RESONANCES AB We investigate the impact of an external magnetic field on ultra-long-range and ultracold Rydberg molecules. The Born-Oppenheimer potential surfaces are analysed and discussed for different values of the magnetic field strength. The magnetic field provides an angular confinement turning a rotational degree of freedom into a vibrational one. We explore the vibrational dynamics and observe a pronounced transition in the level spacing from a linear splitting via an irregular regime to a 2D-harmonic oscillator-like behaviour. Scaling arguments for the dependence of the potential energy surfaces on the field strengths are provided. The occurrence of a monotonic lowering of the magnitude of the electric dipole moment with increasing magnetic field strength is shown. C1 Heidelberg Univ, Inst Phys, D-69120 Heidelberg, Germany. Heidelberg Univ, INF 229, Inst Phys Chem, D-69120 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Lesanovsky, I (reprint author), Heidelberg Univ, Inst Phys, Philosophenweg 12, D-69120 Heidelberg, Germany. EM ilesanov@physi.uni-heidelberg.de; Peter.Schmelcher@pci.uni-heidelberg.de; hrs@cfa.harvard.edu RI Schmelcher, Peter/D-9592-2014; Lesanovsky, Igor/J-6012-2015 OI Schmelcher, Peter/0000-0002-2637-0937; Lesanovsky, Igor/0000-0001-9660-9467 NR 26 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 28 PY 2006 VL 39 IS 4 BP L69 EP L76 DI 10.1088/0953-4075/39/4/L03 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 038JD UT WOS:000237214800003 ER PT J AU Ritson-Williams, R Yotsu-Yamashita, M Paul, VJ AF Ritson-Williams, R Yotsu-Yamashita, M Paul, VJ TI Ecological functions of tetrodotoxin in a deadly polyclad flatworm SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE prey-capture; chemical ecology ID OCTOPUS HAPALOCHLAENA-MACULOSA; RESISTANT SODIUM-CHANNELS; TARICHA-GRANULOSA; PREDATOR; PREY; NEWT; CHAETOGNATHA; VERMICULARIS; BACTERIA; TOXIN AB The deadly neurotoxin tetrodotoxin (TTX) is found in a variety of animal phyla and, because of its toxicity, is most often assumed to deter predation. On the tropical Pacific island of Guam, we found an undescribed flatworm (planocerid sp. 1) that contains high levels of TTX and its analogs. Through ecological experiments, we show that TTXs do not protect these flatworms from some predators but instead are used to capture mobile prey. TTX is known to have multiple ecological functions, which has probably led to its widespread presence among prokaryotes and at least 10 metazoan phyla. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Tohoku Univ, Grad Sch Agr Sci, Aoba Ku, Sendai, Miyagi 9818555, Japan. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM williams@sms.si.edu NR 31 TC 41 Z9 46 U1 0 U2 6 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 28 PY 2006 VL 103 IS 9 BP 3176 EP 3179 DI 10.1073/pnas.0506093103 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 018QU UT WOS:000235780700033 PM 16492790 ER PT J AU Baier-Anderson, C Blount, BC LaKind, JS Naiman, DQ Wilbur, SB Tan, S AF Baier-Anderson, C Blount, BC LaKind, JS Naiman, DQ Wilbur, SB Tan, S TI Estimates of exposures to perchlorate from consumption of human milk, dairy milk, and water, and comparison to current reference dose SO JOURNAL OF TOXICOLOGY AND ENVIRONMENTAL HEALTH-PART A-CURRENT ISSUES LA English DT Article ID SODIUM-IODIDE SYMPORTER; DEVELOPING DEER MICE; FETAL-RAT BRAIN; THYROID-HORMONE; AMMONIUM-PERCHLORATE; POSTNATAL DAY-21; GENE-EXPRESSION; NATIONAL-HEALTH; URINARY IODINE; UNITED-STATES AB To develop an enforceable drinking water standard from a health-based reference dose, sources of exposure and relevant exposure factors across the U. S. population must be considered. Human exposures, expressed as an estimated daily exposure, can be used to evaluate the health protectiveness of a range of potential regulatory values, thus providing a scientific foundation on which decisions can be based. Recent evidence points to detectable levels of perchlorate in milk and other foods. The purpose of this article is to estimate human exposure to perchlorate from ingestion of drinking water, human milk, and dairy milk. Drinking-water exposure was based on a range of possible regulatory values, derived from the recently established reference dose. Exposure to perchlorate from the consumption of milk was based on exploratory Food and Drug Administration dairy milk data, and on additional published perchlorate concentrations in dairy and human milk samples. This effort is exploratory in nature due to the limited data available at this time. However, it is anticipated that these exposure estimates and comparison with the current reference dose will stimulate dialogue and research that will advance the risk assessment for perchlorate. C1 Univ Maryland, Div Environm Epidemiol & Toxicol, Sch Med, Dept Epidemiol & Prevent Med, Baltimore, MD 21201 USA. Ctr Dis Control & Prevent, Div Sci Lab, Natl Ctr Environm Hlth, Atlanta, GA USA. LaKind Associates LLC Catonsville, Catonsville, MD USA. Penn State Univ, Milton S Hershey Med Ctr, Coll Med, Dept Pediat, Hershey, PA 17033 USA. Johns Hopkins Univ, Dept Appl Math & Stat, Baltimore, MD USA. Agcy Tox Subst & Dis Registry, Div Toxicol, Atlanta, GA USA. Smithsonian Inst, Dept Reprod Sci, Washington, DC 20560 USA. RP Baier-Anderson, C (reprint author), Univ Maryland, Div Environm Epidemiol & Toxicol, Sch Med, Dept Epidemiol & Prevent Med, 685 W Baltimore St,MSTF 7-36, Baltimore, MD 21201 USA. EM cbaie001@umaryland.edu NR 45 TC 13 Z9 13 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1528-7394 J9 J TOXICOL ENV HEAL A JI J. Toxicol. Env. Health Part A PD FEB 27 PY 2006 VL 69 IS 4 BP 319 EP 330 DI 10.1080/15287390500323420 PG 12 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 017QQ UT WOS:000235708500005 PM 16407090 ER PT J AU Reinert, JF Harbach, RE Huong, VD AF Reinert, JF Harbach, RE Huong, VD TI Aedes (Finlaya) alongi Galliard and Ngu (Diptera : Culicidae : Aedini): description of the female, redescription of the fourth-instar larva, and reassignment to genus Bothaella Reinert SO ZOOTAXA LA English DT Article DE Bothaella alongi; mosquito; Diptera; Culicidae; Aedini AB The female of Aedes ( Finlaya) alongi is described for the first time and the fourth-instar larva is redescribed in detail. The species is reassigned to Bothaella and compared to other species of the genus. C1 ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL 32608 USA. Smithsonian Inst, Natl Museum Nat Hist, Walter Reed Biosyst Unit, Washington, DC USA. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Natl Inst Malariol Parasitol & Entomol, Hanoi, Vietnam. RP Reinert, JF (reprint author), ARS, Ctr Med Agr & Vet Entomol, USDA, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. EM jreinert@gainesville.usda.ufl.edu; r.harbach@nhm.ac.uk; nimpehanoi@hn.vnn.vn NR 14 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 27 PY 2006 IS 1135 BP 49 EP 55 PG 7 WC Zoology SC Zoology GA 015LA UT WOS:000235551700003 ER PT J AU Childress, L Taylor, JM Sorensen, AS Lukin, MD AF Childress, L Taylor, JM Sorensen, AS Lukin, MD TI Fault-tolerant quantum communication based on solid-state photon emitters SO PHYSICAL REVIEW LETTERS LA English DT Article ID NOISY CHANNELS; SINGLE PHOTONS; CRYPTOGRAPHY; ENTANGLEMENT; TELEPORTATION; PURIFICATION; REPEATERS; ATOM AB We describe a novel protocol for a quantum repeater that enables long-distance quantum communication through realistic, lossy photonic channels. Contrary to previous proposals, our protocol incorporates active purification of arbitrary errors at each step of the protocol using only two qubits at each repeater station. Because of these minimal physical requirements, the present protocol can be realized in simple physical systems such as solid-state single photon emitters. As an example, we show how nitrogen-vacancy color centers in diamond can be used to implement the protocol, using the nuclear and electronic spin to form the two qubits. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Taylor, Jacob/B-7826-2011; Childress, Lilian/H-1359-2012; Sorensen, Anders/L-1868-2013 OI Taylor, Jacob/0000-0003-0493-5594; Childress, Lilian/0000-0002-0507-6392; Sorensen, Anders/0000-0003-1337-9163 NR 26 TC 190 Z9 195 U1 7 U2 26 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 24 PY 2006 VL 96 IS 7 AR 070504 DI 10.1103/PhysRevLett.96.070504 PG 4 WC Physics, Multidisciplinary SC Physics GA 015LY UT WOS:000235554100008 PM 16606069 ER PT J AU McCarthy, MC Yu, Z Sari, L Schaefer, HF Thaddeus, P AF McCarthy, MC Yu, Z Sari, L Schaefer, HF Thaddeus, P TI Monobridged Si2H4 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SILICON-CONTAINING MOLECULES; MICROWAVE-SPECTRA; WAVE; IRC+10216; STATE; HEATS AB The rotational spectrum of a new monobridged isomer of Si2H4, denoted here as H2Si(H)SiH, has been detected by Fourier transform microwave spectroscopy of a supersonic molecular beam through the discharge products of silane. On the basis of high-level coupled cluster theory, this isomer is calculated to lie only 7 kcal/mol above disilene (H2SiSiH2), the most stable isomeric arrangement of Si2H4, and to be fairly polar, with a calculated dipole moment of mu=1.14 D. The rotational spectrum of H2Si(H)SiH exhibits closely spaced line doubling, characteristic of a molecule undergoing high-frequency inversion. Transition state calculations indicate that inversion probably occurs in two steps: migration of the bridged hydrogen atom to form silylsilylene, H3SiSiH, and then internal rotation of the SiH3 group, followed by the reverse process. The potential energy surface for this type of inversion is quite shallow, with a barrier height of only 2-3 kcal/mol. Searches for the rotational lines of silylsilylene, calculated to be of comparable stability to H2Si(H)SiH but about five times less polar (mu=0.23 D), have also been undertaken, so far without success, even though strong lines of H2Si(H)SiH have been detected. The favorable energetics and high polarity of monobridged Si2H4 with respect to either disilene or silylsilylene make it a plausible candidate for radioastronomical detection in sources such as IRC+10216, where comparably large silicon molecules such as SiS, SiC3, and SiC4 have already been discovered. (c) 2006 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Chem, Cambridge, MA 02138 USA. Univ Georgia, Ctr Computat Quantum Chem, Athens, GA 30602 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu OI McCarthy, Michael/0000-0001-9142-0008 NR 29 TC 8 Z9 9 U1 1 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 FEB 21 PY 2006 VL 124 IS 7 AR 074303 DI 10.1063/1.2168150 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 014IP UT WOS:000235473500011 PM 16497032 ER PT J AU Font, AS Johnston, KV Bullock, JS Robertson, BE AF Font, AS Johnston, KV Bullock, JS Robertson, BE TI Chemical abundance distributions of galactic halos and their satellite systems in a Lambda CDM Universe SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : abundances; galaxies : evolution ID DWARF SPHEROIDAL GALAXIES; COLD DARK-MATTER; PROPER-MOTION STARS; METALLICITY DISTRIBUTION; MILKY-WAY; STELLAR HALO; MERGING HISTORY; EARLY EVOLUTION; LOCAL GROUP; OUTER HALO AB We present a cosmologically motivated model for the hierarchical formation of the stellar halo that includes a semianalytic treatment of galactic chemical enrichment coupled to numerical simulations that track the orbital evolution and tidal disruption of satellites. A major motivating factor in this investigation is the observed systematic difference between the chemical abundances of stars in satellite galaxies and those in the Milky Way halo. Specifically, for the same [Fe/H] values, stars in neighboring satellite galaxies display significantly lower [alpha/Fe] ratios than stars in the halo. We find that the observed chemical abundance patterns are a natural outcome of the process of hierarchical assembly of the Galaxy. This result follows because the stellar halo in this context is built up from satellite galaxies accreted early on (more than 8-9 Gyr ago) and enriched in alpha-elements produced in Type II supernovae. In contrast, satellites that still survive today are typically accreted late (within the last 4-5 Gyr) with nearly solar [alpha/Fe] values as a result of contributions from both Type II and Type Ia supernovae. We use our model to investigate the abundance distribution functions (using both [Fe/H] and [alpha/Fe] ratios) for stars in the halo and in surviving satellites. Our results suggest that the shapes and peaks in the abundance distribution functions provide a direct probe of the accretion histories of galaxies. C1 Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA. Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92687 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Font, AS (reprint author), Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA. EM afont@astro.wesleyan.edu; kvj@astro.wesleyan.edu; bullock@uci.edu; brobertson@cfa.harvard.edu RI Bullock, James/K-1928-2015 OI Bullock, James/0000-0003-4298-5082 NR 58 TC 123 Z9 123 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP 585 EP 595 DI 10.1086/498970 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700001 ER PT J AU Bolton, AS Burles, S Koopmans, LVE Treu, T Moustakas, LA AF Bolton, AS Burles, S Koopmans, LVE Treu, T Moustakas, LA TI The Sloan Lens ACS Survey. I. A large spectroscopically selected sample of massive early-type lens galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : formation; galaxies : structure; gravitational lensing ID DIGITAL SKY SURVEY; COLD DARK-MATTER; OPTICAL EINSTEIN RING; NORTH MULTIOBJECT SPECTROGRAPH; GRAVITATIONAL LENS; ELLIPTIC GALAXIES; COSMOLOGICAL PARAMETERS; FUNDAMENTAL PLANE; TARGET SELECTION; BARYONIC INFALL AB The Sloan Lens ACS (SLACS) Survey is an efficient Hubble Space Telescope (HST) Snapshot imaging survey for new galaxy-scale strong gravitational lenses. The targeted lens candidates are selected spectroscopically from the Sloan Digital Sky Survey (SDSS) database of galaxy spectra for having multiple nebular emission lines at a redshift significantly higher than that of the SDSS target galaxy. The SLACS survey is optimized to detect bright early-type lens galaxies with faint lensed sources in order to increase the sample of known gravitational lenses suitable for detailed lensing, photometric, and dynamical modeling. In this paper, the first in a series on the current results of our HST Cycle 13 imaging survey, we present a catalog of 19 newly discovered gravitational lenses, along with nine other observed candidate systems that are either possible lenses, nonlenses, or nondetections. The survey efficiency is thus >= 68%. We also present Gemini 8 m and Magellan 6.5 m integral-field spectroscopic data for nine of the SLACS targets, which further support the lensing interpretation. A new method for the effective subtraction of foreground galaxy images to reveal faint background features is presented. We show that the SLACS lens galaxies have colors and ellipticities typical of the spectroscopic parent sample from which they are drawn (SDSS luminous red galaxies and quiescent MAIN sample galaxies), but are somewhat brighter and more centrally concentrated. Several explanations for the latter bias are suggested. The SLACS survey provides the first statistically significant and homogeneously selected sample of bright early-type lens galaxies, furnishing a powerful probe of the structure of early-type galaxies within the half-light radius. The high confirmation rate of lenses in the SLACS survey suggests consideration of spectroscopic lens discovery as an explicit science goal of future spectroscopic galaxy surveys. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93101 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM bolton@alum.mit.edu; burles@mit.edu; koopmans@astro.rug.nl; tt@physics.ucsb.edu; leonidas@jpl.nasa.gov OI Moustakas, Leonidas/0000-0003-3030-2360 NR 79 TC 227 Z9 227 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP 703 EP 724 DI 10.1086/498884 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700012 ER PT J AU Kallivayalil, N van der Marel, RP Alcock, C Axelrod, T Cook, KH Drake, AJ Geha, M AF Kallivayalil, N van der Marel, RP Alcock, C Axelrod, T Cook, KH Drake, AJ Geha, M TI The proper motion of the Large Magellanic Cloud using HST SO ASTROPHYSICAL JOURNAL LA English DT Article DE Magellanic Clouds ID VARIABILITY-SELECTED QUASARS; INERTIAL REFERENCE SYSTEM; MILKY-WAY; MASS; PROJECT; GALAXY; MACHO; STREAM; QSOS; HALO AB We present a measurement of the systemic proper motion of the Large Magellanic Cloud (LMC) from astrometry with the High Resolution Camera (HRC) of the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). We observed LMC fields centered on 21 background QSOs that were discovered from their optical variability in the MACHO database. The QSOs are distributed homogeneously behind the central few degrees of the LMC. With two epochs of HRC data and a similar to 2 yr baseline, we determine the proper motion of the LMC to better than 5% accuracy: mu(w) = 2: 03 +/- 0: 08 mas yr(-1), and mu(N) = 0:44 +/- 0: 05 mas yr(-1). This is the most accurate proper- motion measurement for any Milky Way satellite thus far. When combined with H I data from the Magellanic Stream, this should provide new constraints on both the mass distribution of the Galactic halo and models of the Stream. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA. Carnegie Observ, Pasadena, CA 91101 USA. RP Kallivayalil, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nkalliva@cfa.harvard.edu; marel@stsci.edu; calcock@cfa.harvard.edu; taxelrod@as.arizona.edu; kcook@llnl.gov; ajd@cacr.caltech.edu; mgeha@ociw.edu NR 39 TC 189 Z9 190 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP 772 EP 785 DI 10.1086/498972 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700018 ER PT J AU Curiel, S Ho, PTP Patel, NA Torrelles, JM Rodriguez, LF Trinidad, MA Canto, J Hernandez, L Gomez, JF Garay, G Anglada, G AF Curiel, S Ho, PTP Patel, NA Torrelles, JM Rodriguez, LF Trinidad, MA Canto, J Hernandez, L Gomez, JF Garay, G Anglada, G TI Large proper motions in the jet of the high-mass YSO Cepheus A HW2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Cepheus A); ISM : jets and outflows; radio continuum : ISM; stars : formation ID LARGE ARRAY OBSERVATIONS; STAR-FORMING REGIONS; OB3 MOLECULAR CLOUD; THERMAL RADIO JET; VLA OBSERVATIONS; VLBI OBSERVATIONS; OUTFLOW; MASERS; SERPENS; DISK AB Using high angular resolution (similar to 0. double prime 25 - 0. double prime 05) Very Large Array (VLA) observations made at 3.6 cm, 1.3 cm, and 7 mm during the period 1991 - 2004, we report the detection of large proper motions in the components of the radio continuum jet associated with the high-mass young stellar object (YSO) HW2 in the star-forming region Cepheus A. The relative proper motions observed for the two main components of the outflow, moving away from the central source in nearly opposite directions, are of the order of 140 mas yr(-1), or similar to 480 km s(-1) at a distance of 725 pc. The proper motions observed in the northeast and southwest lobes are not completely antiparallel, and the central elongated source seems to be changing orientation. We discuss possible scenarios to account for these and other observed characteristics. We also report the detection of a 7 mm compact continuum condensation of emission near the center of the thermal radio continuum jet, which we propose as the location of the exciting star. C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIC, E-08034 Barcelona, Spain. Inst Estud Espacials Catalunya, E-08034 Barcelona, Spain. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Univ Guanajuato, Dept Astron, Guanajuato 36240, Mexico. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. Lab Astrofis Espacial & Fis Fundamental, E-18080 Granada, Spain. Univ Chile, Dept Astron, Santiago, Chile. RP Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70-264, Mexico City 04510, DF, Mexico. EM scuriel@cfa.harvard.edu; pho@cfa.harvard.edu; npatel@cfa.harvard.edu; torrelle@ieec.fcr.es; l.rodriguez@astrosmo.unam.mx; trinidad@astro.ugto.mx; liliana@astroscu.unam.mx; jfg@iaa.es; guido@das.uchile.cl; guillem@iaa.es RI Garay, Guido/H-8840-2013; Gomez, Jose Francisco/D-8392-2016; OI Garay, Guido/0000-0003-1649-7958; Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 41 TC 67 Z9 68 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 FEB 20 PY 2006 VL 638 IS 2 BP 878 EP 886 DI 10.1086/498931 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700026 ER PT J AU Garcia-Alvarez, D Drake, JJ Ball, B Lin, LW Kashyap, VL AF Garcia-Alvarez, D Drake, JJ Ball, B Lin, LW Kashyap, VL TI Evidence of the FIP effect in the coronae of late-type giants SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : activity; stars : coronae; stars : late-type; Sun : corona; X-rays : stars ID X-RAY SPECTROSCOPY; LATE-TYPE STARS; L-SHELL IONS; HERTZSPRUNG-GAP; XMM-NEWTON; EMISSION MEASURE; STELLAR CORONAE; LINE-FORMATION; RED GIANTS; AB-DORADUS AB The stars beta Cet, 31 Com, and mu Vel represent the main stages through which late-type giants evolve during their lifetime (the Hertzsprung gap [31 Com], the rapid braking zone [mu Vel], and the core helium burning ''clump'' phase [beta Cet]). An analysis of their high-resolution Chandra X-ray spectra reveals similar coronal characteristics in terms of both temperature structure and element abundances for the more evolved stars (mu Vel and beta Cet), with slight differences for the ''younger'' giant (31 Com). The coronal temperature structure of 31 Com is significantly hotter, showing a clear peak, while beta Cet and mu Vel show a plateau. beta Cet and mu Vel show evidence for a FIP effect in which coronae are depleted in high-FIP elements relative to their photospheres by a factor of similar to 2. In contrast, 31 Com is characterized by a lack of FIP effect. In other words, neither depletion nor enhancement relative to stellar photospheric values is found. We conclude that the structural changes during the evolution of late-type giants could be responsible for the observed differences in coronal abundances and temperature structure. In particular, the size of the convection zone coupled with the rotation rate seem obvious choices for playing a key role in determining coronal characteristics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garcia-Alvarez, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 84 TC 9 Z9 9 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP 1028 EP 1040 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700041 ER PT J AU Hines, DC Backman, DE Bouwman, J Hillenbrand, LA Carpenter, JM Meyer, MR Kim, JS Silverstone, MD Rodmann, J Wolf, S Mamajek, EE Brooke, TY Padgett, DL Henning, T Moro-Martin, A Stobie, E Gordon, KD Morrison, JE Muzerolle, J Su, KYL AF Hines, DC Backman, DE Bouwman, J Hillenbrand, LA Carpenter, JM Meyer, MR Kim, JS Silverstone, MD Rodmann, J Wolf, S Mamajek, EE Brooke, TY Padgett, DL Henning, T Moro-Martin, A Stobie, E Gordon, KD Morrison, JE Muzerolle, J Su, KYL TI The formation and evolution of planetary systems (FEPS): Discovery of an unusual debris system associated with HD 12039 SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared : stars; planetary systems : protoplanetary disks; stars : individual (HD 12039) ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; TW-HYDRAE ASSOCIATION; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; MULTIBAND IMAGING PHOTOMETER; HF-W CHRONOMETRY; HD 98800; CIRCUMSTELLAR DISKS; VEGA PHENOMENON AB We report the discovery of a debris system associated with the similar to 30 Myr old G3/5V star HD 12039 using Spitzer Space Telescope observations from 3.6-160 mu m. An observed infrared excess (L-IR/L-* = 1 x 10(-4)) above the expected photosphere for lambda greater than or similar to 14 mu m is fit by thermally emitting material with a color temperature of T similar to 110 K, warmer than the majority of debris disks identified to date around Sun-like stars. The object is not detected at 70 mu m with a 3 sigma upper limit 6 times the expected photospheric flux. The spectrum of the infrared excess can be explained by warm, optically thin material comprised of blackbody-like grains of size greater than or similar to 7 mu m that reside in a belt orbiting the star at 4-6 AU. An alternate model dominated by smaller grains, near the blowout size a similar to 0.5 mu m, located at 30-40 AU is also possible but requires the dust to have been produced recently, since such small grains will be expelled from the system by radiation pressure in approximately a few times 10(2) yr. C1 Space Sci Inst, Boulder, CO 80301 USA. NASA, SOFIA, Moffett Field, CA 94035 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. RP Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. OI Su, Kate/0000-0002-3532-5580 NR 106 TC 48 Z9 48 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP 1070 EP 1079 DI 10.1086/498929 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700045 ER PT J AU Bemporad, A Poletto, G Suess, ST Ko, YK Schwadron, NA Elliott, HA Raymond, JC AF Bemporad, A Poletto, G Suess, ST Ko, YK Schwadron, NA Elliott, HA Raymond, JC TI Current sheet evolution in the aftermath of a CME event SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation ID CORONAL MASS EJECTIONS; ELEMENTAL ABUNDANCES; ACTIVE-REGION; SOLAR-FLARE; RECONNECTION; STREAMERS; PLASMA; SPECTROMETER; TEMPERATURE; DIAGNOSTICS AB We report on SOHO UVCS observations of the coronal restructuring following a coronal mass ejection (CME) on 2002 November 26, at the time of a SOHO-Ulysses quadrature campaign. Starting about 1.5 hr after a CME in the northwest quadrant, UVCS began taking spectra at 1.7 R-circle dot, covering emission from both cool and hot plasma. Observations continued, with occasional gaps, for more than 2 days. Emission in the 974.8 angstrom line of [Fe (XVIII)], indicating temperatures above 6 x 10(6) K, was observed throughout the campaign in a spatially limited location. Comparison with EIT images shows the [Fe (XVIII)] emission to overlie a growing post-flare loop system formed in the aftermath of the CME. The emission most likely originates in a current sheet overlying the arcade. Analysis of the [Fe (XVIII)] emission allows us to infer the evolution of physical parameters in the current sheet over the entire span of our observations: in particular, we give the temperature versus time in the current sheet and estimate its density. At the time of the quadrature, Ulysses was directly above the location of the CME and intercepted the ejecta. High ionization state Fe was detected by the Ulysses SWICS throughout the magnetic cloud associated with the CME, although its rapid temporal variation suggests bursty, rather than smooth, reconnection in the coronal current sheet. The SOHO-Ulysses data set provided us with the unique opportunity of analyzing a current sheet structure from its lowest coronal levels out to its in situ properties. Both the remote and in situ observations are compared with predictions of theoretical CME models. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SW Res Inst, San Antonio, TX 78238 USA. RP Univ Florence, Dipartimento Astron & Sci Spazio, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM bemporad@arcetri.astro.it; poletto@arcetri.astro.it OI Bemporad, Alessandro/0000-0001-5796-5653 NR 39 TC 56 Z9 60 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 FEB 20 PY 2006 VL 638 IS 2 BP 1110 EP 1128 DI 10.1086/497529 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RA UT WOS:000235425700049 ER PT J AU Gordon, KD Bailin, J Engelbracht, CW Rieke, GH Misselt, KA Latter, WB Young, ET Ashby, MLN Barmby, P Gibson, BK Hines, DC Hinz, J Krause, O Levine, DA Marleau, FR Noriega-Crespo, A Stolovy, S Thilker, DA Werner, MW AF Gordon, KD Bailin, J Engelbracht, CW Rieke, GH Misselt, KA Latter, WB Young, ET Ashby, MLN Barmby, P Gibson, BK Hines, DC Hinz, J Krause, O Levine, DA Marleau, FR Noriega-Crespo, A Stolovy, S Thilker, DA Werner, MW TI Spitzer MIPS infrared imaging of M31: Further evidence for a spiral-ring composite structure SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31, M32, NGC 205); galaxies : ISM; galaxies : spiral ID HUBBLE-SPACE-TELESCOPE; NEUTRAL HYDROGEN; COSMOLOGICAL SIMULATIONS; ANDROMEDA GALAXY; LOCAL GROUP; BULGE; DISK; CODE; EMISSION; M-31 AB New images of M31 at 24, 70, and 160 mm taken with the Multiband Imaging Photometer for Spitzer (MIPS) reveal the morphology of the dust in this galaxy. This morphology is well represented by a composite of two logarithmic spiral arms and a circular ring (radius similar to 10 kpc) of star formation offset from the nucleus. The two spiral arms appear to start at the ends of a bar in the nuclear region and extend beyond the star-forming ring. As has been found in previous work, the spiral arms are not continuous, but composed of spiral segments. The star-forming ring is very circular except for a region near M32 where it splits. The lack of well-defined spiral arms and the prominence of the nearly circular ring suggest that M31 has been distorted by interactions with its satellite galaxies. Using new dynamical simulations of M31 interacting with M32 and NGC 205, we find that, qualitatively, such interactions can produce an offset, split ring like that seen in the MIPS images. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Gordon, KD (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM kgordon@as.arizona.edu RI Gibson, Brad/M-3592-2015; Barmby, Pauline/I-7194-2016 OI Gibson, Brad/0000-0003-4446-3130; Barmby, Pauline/0000-0003-2767-0090 NR 53 TC 102 Z9 102 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2006 VL 638 IS 2 BP L87 EP L92 DI 10.1086/501046 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013RC UT WOS:000235425900010 ER PT J AU Debnath, U Mukhopadhyay, B Dadhich, N AF Debnath, U Mukhopadhyay, B Dadhich, N TI Spacetime curvature coupling of spinors in early universe: Neutrino asymmetry and a possible source of baryogenesis SO MODERN PHYSICS LETTERS A LA English DT Article DE neutrino asymmetry; early universe; anisotropic spacetime; CPT violation ID CPT VIOLATION; INFLATIONARY UNIVERSE; GRAVITATIONAL-FIELD; SPIN-1/2 PARTICLE; STANDARD MODEL; BLACK-HOLES; COSMOLOGY; FLATNESS; HORIZON AB It is well known that when a fermion propagates in curved spacetime, its spin couples to the curvature of background spacetime. We propose that this interaction for neutrinos propagating in early curved universe could give rise to a new set of dispersion relations and then neutrino asymmetry at equilibrium. We demonstrate this with the Bianchi models which describe the homogeneous but anisotropic and axially symmetric universe. If the lepton number violating processes freeze out at 10(-37) s when temperature T similar to 10(15) GeV, neutrino asymmetry of the order of 10(-10) can be generated. A net baryon asymmetry of the same magnitude can thus be generated from this lepton asymmetry either by a CUT B - L symmetry or by the electroweak sphaleron processes which have B + L symmetry. C1 Jadavpur Univ, Dept Math, Kolkata 700032, W Bengal, India. Bengal Engn & Sci Univ, Dept Math, Sibpur 711103, Howrah, India. Harvard Smithsonian Ctr Astrophys, Div Theory, Cambridge, MA 02138 USA. Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. RP Debnath, U (reprint author), Jadavpur Univ, Dept Math, Kolkata 700032, W Bengal, India. EM ujjal@iucaa.ernet.in; bmukhopa@cfa.harvard.edu; nkd@iucaa.ernet.in NR 45 TC 21 Z9 21 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 EI 1793-6632 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD FEB 20 PY 2006 VL 21 IS 5 BP 399 EP 408 DI 10.1142/S0217732306019542 PG 10 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 026WL UT WOS:000236373700003 ER PT J AU Frazier, J AF Frazier, J TI Biosphere reserves and the "Yucatan" syndrome: another look at the role of NGOs SO LANDSCAPE AND URBAN PLANNING LA English DT Article; Proceedings Paper CT 61st Annual Meeting of the Society-for-Applied-Anthropology CY MAR 28-APR 01, 2001 CL Merida, MEXICO DE conservation; development; globalization; imperialism ID CONSERVATION; PERSPECTIVE; DISCOURSE; MOVEMENT; TREE AB After centuries of cultural and economic conquest of the Americas by European and Euro-Arnerican conquistadors, contemporary rhetoric in ex-colonial powers heralds the decline of material and ideological imperialism. Instead, it is purported that today's world is peopled by a great brotherhood, with the more affluent striving to relieve their less fortunate, underdeveloped kith. This conviction is inherent in organizations which dispense money, information, training, and other resources in the name of community development and endangered species and environmental conservation. What is rarely perceived - and practically never said - is that these "benevolent" foreign aid activities typically result in the concentration of resources and power in the hands of a few, the building of empires, and the compounding of already difficult situations, counter-productive to stated objectives. The Yucatan Peninsula is a classic case of persistent imperialism: the geographic name is a corruption of the Mayan "matan cub a than" ("I do not understand you"), while contemporary development and conservation programs habitually exhibit cultural ignorance and dominance. This paper explores a diverse literature on non-govern mental organizations, reflects on likely consequences of cultural dominance, and implores professional anthropologists to be adventurous in propagating anthropological knowledge relevant to environmental protection. (c) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Frazier, J (reprint author), Smithsonian Inst, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM frazierja@crc.si.edu NR 121 TC 3 Z9 3 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-2046 J9 LANDSCAPE URBAN PLAN JI Landsc. Urban Plan. PD FEB 15 PY 2006 VL 74 IS 3-4 BP 313 EP 333 DI 10.1016/j.landurbplan.2004.09.010 PG 21 WC Ecology; Environmental Studies; Geography; Geography, Physical; Urban Studies SC Environmental Sciences & Ecology; Geography; Physical Geography; Urban Studies GA 985CW UT WOS:000233354700010 ER PT J AU Broderick, AE AF Broderick, AE TI Radiative transfer along rays in curved space-times SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; radiative transfer; relativity ID COVARIANT MAGNETOIONIC THEORY; BLACK-HOLE; TRANSPORT; SPECTRA AB Radiative transfer in curved space-times has become increasingly important to understanding high-energy astrophysical phenomena and testing general relativity in the strong field limit. The equations of radiative transfer are physically equivalent to the Boltzmann equation, where the latter has the virtue of being covariant. We show that by a judicious choice of the basis of the phase space, it is generally possible to make the momentum derivatives in the Boltzmann equation vanish along an arbitrary (including non-geodesic) path, thus reducing the problem of radiative transfer along a ray to a path integral in coordinate space. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu NR 17 TC 15 Z9 15 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 11 PY 2006 VL 366 IS 1 BP L10 EP L12 DI 10.1111/j.1745-3933.2005.00120.x PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 006DW UT WOS:000234876700003 ER PT J AU Chazelas, B Brachet, F Borde, P Mennesson, B Ollivier, M Absil, O Labeque, A Valette, C Leger, A AF Chazelas, B Brachet, F Borde, P Mennesson, B Ollivier, M Absil, O Labeque, A Valette, C Leger, A TI Instrumental stability requirements for exoplanet detection with a nulling interferometer: variability noise as a central issue SO APPLIED OPTICS LA English DT Article ID EXTRASOLAR PLANETS AB We revisit the nulling interferometer performances that are needed for direct detection and the spectroscopic analysis of exoplanets, e.g., with the DARWIN [European Space Agency-SCI 12 (2000)] or TPF-I [JPL Publ. 05-5, (2005)] missions. Two types of requirement are found, one concerning the mean value of the instrumental nulling function < nl(lambda)> and another regarding its stability. The stress is usually put on the former. It is stringent at short wavelengths but somewhat relaxed at longer wavelengths. The latter, which we call the variability noise condition, does not usually receive enough attention. It is required regardless of telescope size and stellar distance. The results from three nulling experiments performed in laboratories around the world are reported and compared with the requirements. All three exhibit 1/f noise that is incompatible with the performances required by the mission. As pointed out by Lay [Appl. Opt. 43, 6100-6123 (2004)], this stability problem is not fully solved by modulation techniques. Adequate solutions must be found that are likely to include servo systems using the stellar signal itself as a reference and internal metrology with high stability. (c) 2006 Optical Society of America. C1 Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. RP Chazelas, B (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM Alain.Leger@ias.u-psud.fr OI Absil, Olivier/0000-0002-4006-6237 NR 15 TC 18 Z9 18 U1 1 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD FEB 10 PY 2006 VL 45 IS 5 BP 984 EP 992 DI 10.1364/AO.45.000984 PG 9 WC Optics SC Optics GA 013CO UT WOS:000235387400021 PM 16512542 ER PT J AU Lidz, A Heitmann, K Hui, L Habib, S Rauch, M Sargent, WLW AF Lidz, A Heitmann, K Hui, L Habib, S Rauch, M Sargent, WLW TI Tightening constraints from the Ly alpha forest with the flux probability distribution function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; intergalactic medium; large-scale structure of universe; quasars : absorption lines ID TEMPERATURE-DENSITY RELATION; POWER SPECTRUM; INTERGALACTIC MEDIUM; COSMOLOGICAL PARAMETERS; MASS FLUCTUATIONS; STATISTICS; ABSORPTION; EVOLUTION; MODEL; SIMULATIONS AB The analysis of the Ly alpha forest of absorption lines in quasar spectra has emerged as a potentially powerful technique to constrain the linear matter power spectrum. In most previous work, the amplitude of the ionizing background was fixed by calibrating simulations to match the observed mean transmitted flux in the Ly alpha forest. This procedure is undesirable in principle, as it requires the estimation of the unabsorbed quasar continuum level, a difficult undertaking subject to various sources of systematic error and bias. We suggest an alternative approach based on measuring the one-point probability distribution function (pdf) of the fluctuations in the flux about the mean, relative to the mean, i.e., the pdf of delta(f) = ( f - < f >)/< f >. This statistic, while sensitive to the amplitude of the ionizing background, has the virtue that its measurement does not require an estimate of the unabsorbed continuum level. We present a measurement of the pdf of delta(f) from seven Keck HIRES spectra, spanning a redshift range of z = 2.2 - 4.4. To illustrate that our method is useful, we compare our measurements of the pdf of delta(f) and measurements of the flux power spectrum from Croft et al. at z = 2.72, with cosmological simulations. From this comparison, we obtain constraints on the mean transmission in the Ly alpha forest, the slope of the temperature-density relation, as well as the amplitude and slope of the mass power spectrum. Our methodology is useful for obtaining more precise constraints with larger data samples from the Sloan Digital Sky Survey (SDSS). C1 Columbia Univ, Dept Phys, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. Univ Calif Los Angeles, ISRI, ISR Div, Los Alamos, NM 87545 USA. Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. Carnegie Observ, Pasadena, CA 91101 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Lidz, A (reprint author), Columbia Univ, Dept Phys, New York, NY 10027 USA. EM alidz@cfa.harvard.edu; heitmann@lanl.gov; lhui@asxtro.columnia.edu; habib@lanl.gov; mr@ociw.edu; wws@phobos.caltech.edu NR 54 TC 30 Z9 30 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2006 VL 638 IS 1 BP 27 EP 44 DI 10.1086/498699 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100003 ER PT J AU Kondratko, PT Greenhill, LJ Moran, JM Lovell, JEJ Kuiper, TBH Jauncey, DL Cameron, LB Gomez, JF Garcia-Miro, C Moll, E de Gregorio-Monsalvo, I Jimenez-Bailon, E AF Kondratko, PT Greenhill, LJ Moran, JM Lovell, JEJ Kuiper, TBH Jauncey, DL Cameron, LB Gomez, JF Garcia-Miro, C Moll, E de Gregorio-Monsalvo, I Jimenez-Bailon, E TI Discovery of water maser emission in eight AGNs with 70 m antennas of NASA'S Deep Space Network SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (AM 2158-380 NED02, IC 0184, NGC 0235A, NGC 0613, NGC 3393, NGC 4293, NGC 5495, VII Zw 073); galaxies : Seyfert; ISM : jets and outflows; ISM : molecules; masers ID ACTIVE GALACTIC NUCLEI; DWARF SEYFERT NUCLEI; PARSEC-SCALE JET; H2O MASER; NEARBY GALAXIES; CIRCINUS GALAXY; ACCRETION DISK; BLACK-HOLE; X-RAY; SEARCH AB We report the discovery of water maser emission in eight active galactic nuclei (AGNs) with the 70 m NASA Deep Space Network (DSN) antennas at Tidbinbilla, Australia, and Robledo, Spain. The positions of the newly discovered masers, measured with the VLA, are consistent with the optical positions of the host nuclei to within 1 sigma(0 ''.3 radio and 1 ''.3 optical) and most likely mark the locations of the embedded central engines. The spectra of two sources, NGC 3393 and NGC 5495, display the characteristic spectral signature of emission from an edge-on accretion disk, with orbital velocities of similar to 600 and similar to 400 km s(-1), respectively. In a survey with DSN facilities of 630 AGNs selected from the NASA Extragalactic Database, we have discovered a total of 15 water maser sources. The resulting incidence rate of maser emission among nearby (v(sys) < 7000 km s(-1)) Seyfert 1.8-2.0 and LINER systems is similar to 10% for a typical rms noise level of similar to 14 mJy over 1.3 km s(-1) spectral channels. As a result of this work, the number of nearby AGNs (v(sys) < 7000 km s(-1)) observed with < 20 mJy rms noise has increased from 130 to 449. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. Canberra Deep Space Commun Complex, Paddys Creek, ACT 2609, Australia. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. NASA, INTA, E-28008 Madrid, Spain. INTA, Lab Astrofis Espac & Fis Fundamental, E-28080 Madrid, Spain. RP Kondratko, PT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pkondrat@cfa.harvard.edu RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Moran, James/0000-0002-3882-4414 NR 42 TC 40 Z9 41 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2006 VL 638 IS 1 BP 100 EP 105 DI 10.1086/498641 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100008 ER PT J AU Enoch, ML Young, KE Glenn, J Evans, NJ Golwala, S Sargent, AI Harvey, P Aguirre, J Goldin, A Haig, D Huard, TL Lange, A Laurent, G Maloney, P Mauskopf, P Rossinot, P Sayers, J AF Enoch, ML Young, KE Glenn, J Evans, NJ Golwala, S Sargent, AI Harvey, P Aguirre, J Goldin, A Haig, D Huard, TL Lange, A Laurent, G Maloney, P Mauskopf, P Rossinot, P Sayers, J TI Bolocam survey for 1.1 mm dust continuum emission in the c2d legacy clouds. I. Perseus SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (Perseus); stars : formation ID MASS STAR-FORMATION; PRE-PROTOSTELLAR CORES; BARNARD-1 DARK CLOUD; MOLECULAR CLOUDS; INTERSTELLAR EXTINCTION; INITIAL CONDITIONS; DENSITY STRUCTURE; CARBON-MONOXIDE; CLUSTER IC-348; PROTOSTARS AB We have completed a 1.1 mm continuum survey of 7.5 deg(2) of the Perseus Molecular Cloud using Bolocam at the Caltech Submillimeter Observatory. This represents the largest millimeter or submillimeter continuum map of Perseus to date. Our map covers more than 30,000 3100 (FWHM) resolution elements to a 1 sigma rms of 15 mJy beam(-1). We detect a total of 122 cores above a 5 sigma point-source mass detection limit of 0.18 M-circle dot, assuming a dust temperature of TD = 10 K, 60 of which are new millimeter or submillimeter detections. The 1.1 mm mass function is consistent with a broken power law of slope alpha 1 = 1.3 ( 0.5 M-circle dot < M < 2.5 M-circle dot) and alpha 2 = 2.6 ( M > 2.5 M-circle dot), similar to the local initial mass function slope (alpha(1)=1.6, M < 1M(circle dot); alpha(2) = 2.7M > 1M(circle dot)). No more than 5% of the total cloud mass is contained in discrete 1.1 mm cores, which account for a total mass of 285 M-circle dot. We suggest an extinction threshold for millimeter cores of AV similar to 5 mag, based on our calculation of the probability of finding a 1.1 mm core as a function of AV. Much of the cloud is devoid of compact millimeter emission; despite the significantly greater area covered compared to previous surveys, only 5 - 10 of the newly identified sources lie outside previously observed areas. The two-point correlation function confirms that dense cores in the cloud are highly structured, with significant clustering on scales as large as 2 x 10(5) AU. Our 1.1 mm emission survey reveals considerably denser, more compact material than maps in other column density tracers such as (CO)-C-13 and A(V), although the general morphologies are roughly consistent. These 1.1 mm results, especially when combined with recently acquired c2d Spitzer Legacy data, will provide a census of dense cores and protostars in Perseus and improve our understanding of the earliest stages of star formation in molecular clouds. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Cardiff Wales, Cardiff, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Enoch, ML (reprint author), CALTECH, Div Phys Math & Astron, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM menoch@astro.caltech.edu; kaisa@astro.as.utexas.edu; jason.glenn@colorado.edu NR 77 TC 218 Z9 218 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2006 VL 638 IS 1 BP 293 EP 313 DI 10.1086/498678 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100027 ER PT J AU D'Alessio, P Calvet, N Hartmann, L Franco-Hernandez, R Servin, H AF D'Alessio, P Calvet, N Hartmann, L Franco-Hernandez, R Servin, H TI Effects of dust growth and settling in T Tauri disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : formation; stars : pre-main-sequence ID SPECTRAL ENERGY-DISTRIBUTIONS; 2-DIMENSIONAL RADIATIVE-TRANSFER; AURIGA MOLECULAR CLOUD; HERBIG AE/BE STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; YOUNG OBJECTS; CIRCUMSTELLAR DISKS; PROTOSTELLAR ENVELOPES; HYDRAE AB We present self-consistent disk models of T Tauri stars that include a parameterized treatment of dust settling and grain growth, building on techniques developed in a series of papers by D'Alessio et al. The models incorporate depleted distributions of dust in upper disk layers along with larger sized particles near the disk midplane, which are expected theoretically and, as we suggested earlier, are necessary to account for millimeter-wave emission, SEDs, scattered light images, and silicate emission features simultaneously. By comparing the models with recent mid- and near-IR observations, we find that the dust-to-gas mass ratio of small grains at the upper layers should be < 10% of the standard value. The grains that have disappeared from the upper layers increase the dust-to-gas mass ratio of the disk interior; if those grains grow to maximum sizes of the order of millimeters during the settling process, then both the millimeter-wave fluxes and spectral slopes can be consistently explained. Depletion and growth of grains can also enhance the ionization of upper layers, increasing the possibility of the magnetorotational instability for driving disk accretion. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron Astrofis, Morelia 58089, Michoacan, Mexico. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP D'Alessio, P (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron Astrofis, Apartado Postal 72,Xangari, Morelia 58089, Michoacan, Mexico. EM p.dalessio@astrosmo.unam.mx; ncalvet@umich.edu; lhartm@umich.edu; r.franco@astrosmo.unam.mx NR 62 TC 214 Z9 214 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2006 VL 638 IS 1 BP 314 EP 335 DI 10.1086/498861 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100028 ER PT J AU Bloom, JS Prochaska, JX Pooley, D Blake, CH Foley, RJ Jha, S Ramirez-Ruiz, E Granot, J Filippenko, AV Sigurdsson, S Barth, AJ Chen, HW Cooper, MC Falco, EE Gal, RR Gerke, BF Gladders, MD Greene, JE Hennanwi, J Ho, LC Hurley, K Koester, BP Li, W Lubin, L Newman, J Perley, DA Squires, GK Wood-Vasey, WM AF Bloom, JS Prochaska, JX Pooley, D Blake, CH Foley, RJ Jha, S Ramirez-Ruiz, E Granot, J Filippenko, AV Sigurdsson, S Barth, AJ Chen, HW Cooper, MC Falco, EE Gal, RR Gerke, BF Gladders, MD Greene, JE Hennanwi, J Ho, LC Hurley, K Koester, BP Li, W Lubin, L Newman, J Perley, DA Squires, GK Wood-Vasey, WM TI Closing in on a short-hard burst progenitor: Constraints from early-time optical imaging and spectroscopy of a possible host galaxy of GRB 050509b SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays : bursts ID GAMMA-RAY BURSTS; BLACK-HOLE BINARIES; COALESCING NEUTRON-STARS; DIGITAL SKY SURVEY; SHORT-DURATION; AFTERGLOW OBSERVATIONS; BATSE OBSERVATIONS; SUPERNOVA 1993J; GIANT FLARE; MERGERS AB The localization of the short-duration, hard-spectrum gamma-ray burst GRB 050509b by the Swift satellite was a watershed event. We report the discovery of the probable host galaxy, a bright elliptical galaxy at z = 0.2248. This is the first known redshift and host of a short-hard GRB and shows that at least some short-hard GRBs are cosmological in origin. We began imaging the GRB field 8 minutes after the burst and continued for 8 days. We present a reanalysis of the XRT afterglow and report the absolute position of the GRB. Based on positional coincidences, the GRB and the elliptical are likely to be physically related, unlike any known connection between a long-duration GRB and an early-type galaxy. Similarly unique, GRB 050509b likely also originated from within a rich cluster of galaxies with detectable diffuse X-ray emission. We demonstrate that while the burst was underluminous, the ratio of the blast wave energy to the gamma-ray energy is consistent with that of long-duration GRBs. Based on this analysis, on the location of the GRB (40 +/- 13 kpc from the putative host), on the galaxy type (elliptical), and the lack of a coincident supernova, we suggest that there is now observational support for the hypothesis that short-hard bursts arise during the merger of a compact binary. We limit the properties of any Li-Paczynski "minisupernova'' that is predicted to arise on similar to 1 day timescales. Other progenitor models are still viable, and new Swift bursts will undoubtedly help to further clarify the progenitor picture. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Adv Study, Princeton, NJ 08540 USA. Stanford Univ, KIPAC, Stanford, CA 94309 USA. Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Inst Nucl & Particle Astrophys, Berkeley, CA 94720 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Bloom, JS (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Barth, Aaron/0000-0002-3026-0562 NR 143 TC 221 Z9 223 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2006 VL 638 IS 1 BP 354 EP 368 DI 10.1086/498107 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100031 ER EF