FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Granot, J Ramirez-Ruiz, E Taylor, GB Eichler, D Lyubarsky, YE Wijers, RAMJ Gaensler, BM Gelfand, JD Kouveliotou, C AF Granot, J Ramirez-Ruiz, E Taylor, GB Eichler, D Lyubarsky, YE Wijers, RAMJ Gaensler, BM Gelfand, JD Kouveliotou, C TI Diagnosing the outflow from the SGR 1806-20 giant flare with radio observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM : bubbles; pulsars : individual (SGR 1806-20); stars : flare; stars : neutron; stars : winds, outflows ID SGR 1806-20; MAGNETAR SGR-1806-20; AFTERGLOW; DISTANCE AB On 2004 December 27, the soft gamma repeater (SGR) 1806-20 emitted the brightest giant flare (GF) ever detected from an SGR. This burst of energy, which resulted in an ( isotropic) energy release similar to 100 times greater than the only two other known SGR GFs, was followed by a very bright, fading radio afterglow. Extensive follow-up radio observations provided a wealth of information with unprecedented astrometric precision, revealing the temporal evolution of the source size, along with densely sampled light curves and spectra. Here we expand on our previous work on this source, by explaining these observations within one self-consistent dynamical model. In this scenario, the early radio emission is due to the outflow ejected during the GF energizing a thin shell surrounding a preexisting cavity, where the observed steep temporal decay of the radio emission seen beginning on day 9 is attributed to the adiabatic cooling of the shocked shell. The shocked ejecta and external shell move outward together, driving a forward shock into the ambient medium, and are eventually decelerated by a reverse shock. As we show in a separate work by Gelfand and coworkers, the radio emission from the shocked external medium naturally peaks when significant deceleration occurs and then decays relatively slowly. The dynamical modeling of the collision between the ejecta and the external shell, together with the observed evolution of the source size ( which is nicely reproduced in our model), suggests that most of the energy in the outflow was in mildly relativistic material, with an initial expansion velocity v/c <= d(15)(1 + d(15)(2))(-1/2) similar to 0.7, for a distance of 15d(15) kpc to SGR 1806-20. An initially highly relativistic outflow would not have produced a long coasting phase at a mildly relativistic expansion velocity, as was observed. C1 Stanford Univ, KIPAC, Stanford, CA 94309 USA. Inst Adv Study, Princeton, NJ 08540 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RP Granot, J (reprint author), Stanford Univ, KIPAC, POB 20450,MS 29, Stanford, CA 94309 USA. EM granot@slac.stanford.edu RI Gaensler, Bryan/F-8655-2010; LYUBARSKY, YURY/F-2362-2012; Gelfand, Joseph/F-1110-2015; OI Gelfand, Joseph/0000-0003-4679-1058; Wijers, Ralph/0000-0002-3101-1808; Gaensler, Bryan/0000-0002-3382-9558 NR 17 TC 35 Z9 35 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 391 EP 396 DI 10.1086/497680 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100034 ER PT J AU Borde, PJ Traub, WA AF Borde, PJ Traub, WA TI High-contrast imaging from space: Speckle nulling in a low-aberration regime SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : adaptive optics; planetary systems; techniques : high angular resolution ID TERRESTRIAL PLANETS; DEFORMABLE MIRROR; CORONAGRAPH; TELESCOPES; IMAGES; COMPANION AB High-contrast imaging from space must overcome two major noise sources to successfully detect a terrestrial planet angularly close to its parent star: photon noise from diffracted starlight and speckle noise from starlight scattered by instrumentally generated wave front perturbation. Coronagraphs tackle only the photon noise contribution by reducing diffracted starlight at the location of a planet. Speckle noise should be addressed with adaptive optics systems. Following the tracks of Malbet, Yu, and Shao, we develop in this paper two analytical methods for wave front sensing and control that aims at creating "dark holes,'' i.e., areas of the image plane cleared of speckles, assuming an ideal coronagraph and small aberrations. The first method, "speckle field nulling,'' is a fast FFT-based algorithm that requires the deformable-mirror influence functions to have identical shapes. The second method, "speckle energy minimization,'' is more general and provides the optimal deformable mirror shape via matrix inversion. With an N x N deformable mirror, the size of the matrix to be inverted is either N-2 x N-2 in the general case or only N; N if the influence functions can be written as the tensor product of two one-dimensional functions. Moreover, speckle energy minimization makes it possible to trade off some of the dark hole area against an improved contrast. For both methods, complex wave front aberrations (amplitude and phase) are measured using just three images taken with the science camera (no dedicated wave front sensing channel is used); therefore, there are no noncommon path errors. We assess the theoretical performance of both methods with numerical simulations including realistic speckle noise and experimental influence functions. We find that these speckle-nulling techniques should be able to improve the contrast by several orders of magnitude. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM pborde@cfa.harvard.edu; wtraub@jpl.nasa.gov NR 24 TC 119 Z9 119 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 488 EP 498 DI 10.1086/498669 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SF UT WOS:000235132100043 ER PT J AU Broderick, AE Narayan, R AF Broderick, AE Narayan, R TI On the nature of the compact dark mass at the galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy : center; gravitational lensing; infrared : general; submillimeter ID SAGITTARIUS-A-ASTERISK; BLACK-HOLE; SGR-A; ACCRETION FLOW; EVENT-HORIZON; MILKY-WAY; GALAXY; STARS; SIZE AB We consider a model in which Sgr A*, the 3.7 x 10 (6) M-circle dot supermassive black hole candidate at the Galactic center, is a compact object with a thermally emitting surface. For very compact surfaces within the photon orbit, the thermal assumption is likely to be a good approximation because of the large number of rays that are strongly gravitationally lensed back onto the surface. Given the very low quiescent luminosity of Sgr A* in the near-infrared, the existence of a hard surface, even in the limit in which the radius approaches the horizon, places a severe constraint on the steady mass accretion rate onto the source: M <= 10(-12) M-circle dot yr(-1). This limit is well below the minimum accretion rate needed to power the observed submillimeter luminosity of Sgr A*: M > yr(-1) M-circle dot yr(-1) . We thus argue that Sgr A* does not have a surface, i. e., that it must have an event horizon. The argument could be made more restrictive by an order of magnitude with microarcsecond resolution imaging, e. g., with submillimeter very long baseline interferometry. long baseline interferometry. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Mail Stop 51,60 Garden St, Cambridge, MA 02138 USA. EM abroderick@cfa.harvard.edu; rnarayan@cfa.harvard.edu NR 28 TC 58 Z9 58 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 L21 EP L24 DI 10.1086/500930 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SH UT WOS:000235132400006 ER PT J AU Kornicker, LS AF Kornicker, LS TI Authorship and publication date of the Palaeozoic genera Cypridinella, Cypridellina, Sulcuna, Rhombina, and Offa (Ostracoda : Myodocopa) SO ZOOTAXA LA English DT Article DE Sulcuna; Jones; Authorship; Ostracoda; Myodocopa; Palaeozoic AB Authorship and publication date of the Palaeozoic genera Cypridinella, Cypridellina, Rhombina, Sulcuna, and Offa have been attributed in the literature to either Jones 1873a, Jones & Kirkby, 1874, or Jones, Kirkby, and Brady, 1874, or 1884 (see Kornicker, 2001). Kornicker (2001) concluded that the correct authorship and publication date of the five genera are Jones, 1873a. Becker (2004) disputed this and argued that the correct authorship and publication date of the first four genera are Jones and Kirkby, 1874 (Offa not mentioned), centering his argument on the genus Sulcuna. On June 10, 2005, I forwarded a request to the International Commission on Zoological Nomenclature (ICZN) requesting a ruling on the identity of the author of the Palaeozoic genus Sulcuna. An answering letter received in August 2005 from the ICZN Secretariat (Fig. 1) stated that Jones (1873a) should be credited as the author of the genus Sulcuna. C1 Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Kornicker, LS (reprint author), Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, MRC 163, Washington, DC 20013 USA. EM kornickl@si.edu NR 13 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 10 PY 2006 IS 1125 BP 39 EP 43 PG 5 WC Zoology SC Zoology GA 010WX UT WOS:000235229700002 ER PT J AU Collin, R Wonham, MJ Barr, KR AF Collin, R Wonham, MJ Barr, KR TI Crepidula convexa Say, 1822 (Caenogastropoda : Calyptraeidae) in Washington State, USA SO AMERICAN MALACOLOGICAL BULLETIN LA English DT Article DE Gastropod taxonomy; cryptic species; introductions ID GASTROPODA; PHYLOGENY AB With the increasing attention to the expansion and impact of invasive species, it has become more important to document carefully new observations of introduced species. Here we document the occurrence of Crepidula convexa, a species from the north Atlantic, in Washington State, U.S.A. DNA sequence data suggest that the animals in Washington originated from the northern part of the species's native range. C1 Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. Univ Washington, Dept Zool, Seattle, WA 98195 USA. Univ SW Louisiana, Dept Biol, Lafayette, LA 70504 USA. RP Collin, R (reprint author), Univ Alberta, CAB 632, Edmonton, AB T6G 2G1, Canada. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 18 TC 6 Z9 6 U1 0 U2 2 PU AMER MALACOLOGICAL SOC, INC PI WILMINGTON PA DELAWARE MUSEUM NATURAL HISTORY, BOX 3937, WILMINGTON, DE 19807-0937 USA SN 0740-2783 J9 AM MALACOL BULL JI Am. Malacol. Bull. PD FEB 9 PY 2006 VL 21 IS 1-2 BP 113 EP 116 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 041TJ UT WOS:000237478500014 ER PT J AU do Amaral, FSR Miller, MJ Silveira, LF Bermingham, E Wajntal, A AF do Amaral, FSR Miller, MJ Silveira, LF Bermingham, E Wajntal, A TI Polyphyly of the hawk genera Leucopternis and Buteogallus (Aves, Accipitridae): multiple habitat shifts during the Neotropical buteonine diversification SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID MITOCHONDRIAL-DNA; HISTORICAL BIOGEOGRAPHY; LOWLAND FOREST; PHYLOGENETIC INFERENCE; ECOLOGICAL GRADIENTS; BIRD-LIFE; SEQUENCE; PSITTACIDAE; SPECIATION; DIVERSITY AB Background: The family Accipitridae ( hawks, eagles and Old World vultures) represents a large radiation of predatory birds with an almost global distribution, although most species of this family occur in the Neotropics. Despite great morphological and ecological diversity, the evolutionary relationships in the family have been poorly explored at all taxonomic levels. Using sequences from four mitochondrial genes (12S, ATP8, ATP6, and ND6), we reconstructed the phylogeny of the Neotropical forest hawk genus Leucopternis and most of the allied genera of Neotropical buteonines. Our goals were to infer the evolutionary relationships among species of Leucopternis, estimate their relationships to other buteonine genera, evaluate the phylogenetic significance of the white and black plumage patterns common to most Leucopternis species, and assess general patterns of diversification of the group with respect to species' affiliations with Neotropical regions and habitats. Results: Our molecular phylogeny for the genus Leucopternis and its allies disagrees sharply with traditional taxonomic arrangements for the group, and we present new hypotheses of relationships for a number of species. The mtDNA phylogenetic trees derived from analysis of the combined data posit a polyphyletic relationship among species of Leucopternis, Buteogallus and Buteo. Three highly supported clades containing Leucopternis species were recovered in our phylogenetic reconstructions. The first clade consisted of the sister pairs L. lacernulatus and Buteogallus meridionalis, and Buteogallus urubitinga and Harpyhaliaetus coronatus, in addition to L. schistaceus and L. plumbeus. The second clade included the sister pair Leucopternis albicollis and L. occidentalis as well as L. polionotus. The third lineage comprised the sister pair L. melanops and L. kuhli, in addition to L. semiplumbeus and Buteo buteo. According to our results, the white and black plumage patterns have evolved at least twice in the group. Furthermore, species found to the east and west of the Andes (cis-Andean and trans-Andean, respectively) are not reciprocally monophyletic, nor are forest and non-forest species. Conclusion: The polyphyly of Leucopternis, Buteogallus and Buteo establishes a lack of concordance of current Accipitridae taxonomy with the mtDNA phylogeny for the group, and points to the need for further phylogenetic analysis at all taxonomic levels in the family as also suggested by other recent analyses. Habitat shifts, as well as cis- and trans-Andean disjunctions, took place more than once during buteonine diversification in the Neotropical region. Overemphasis of the black and white plumage patterns has led to questionable conclusions regarding the relationships of Leucopternis species, and suggests more generally that plumage characters should be used with considerable caution in the taxonomic evaluation of the Accipitridae. C1 Univ Sao Paulo, Dept Genet & Biol Evolut, BR-05508900 Sao Paulo, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Univ Sao Paulo, Dept Zool, BR-05508900 Sao Paulo, Brazil. RP do Amaral, FSR (reprint author), Univ Sao Paulo, Dept Genet & Biol Evolut, Rua Matao 277,Cidade Univ, BR-05508900 Sao Paulo, Brazil. EM fabioraposo@hotmail.com; millerma@si.edu; lfsilvei@usp.br; bermingb@si.edu; aniwa@usp.br RI Miller, Matthew/B-4560-2008; Raposo do Amaral, Fabio/B-9817-2012; Silveira, Luis/F-8337-2012 OI Miller, Matthew/0000-0002-2939-0239; Raposo do Amaral, Fabio/0000-0002-1133-3789; Silveira, Luis/0000-0003-2576-7657 NR 80 TC 7 Z9 7 U1 1 U2 6 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD FEB 7 PY 2006 VL 6 AR 10 DI 10.1186/1471-2148-6-10 PG 10 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 025OK UT WOS:000236275700001 ER PT J AU Yoshino, K Thorne, AP Murray, JE Cheung, ASC Wong, AL Imajo, T AF Yoshino, K Thorne, AP Murray, JE Cheung, ASC Wong, AL Imajo, T TI The application of a vacuum-ultraviolet Fourier transform spectrometer and synchrotron-radiation source to measurements of bands of NO. VII. The final report SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ABSORPTION CROSS-SECTIONS; SCHUMANN-RUNGE BANDS; NITRIC-OXIDE; OSCILLATOR-STRENGTHS; HIGH-RESOLUTION; PREDISSOCIATION; MOLECULE; BETA; FLUORESCENCE; SPECTROSCOPY AB Photoabsorption measurements of NO bands have been made by vacuum-ultraviolet Fourier transform spectrometry with a resolution of 0.12 cm(-1) in the wavelength region of 166.2-196.2 nm. Accurate line positions are obtained for the delta(upsilon,0) bands with upsilon=2, 3, the epsilon(upsilon,0) bands with upsilon=2, 3, and the beta(upsilon,0) bands with upsilon=10,12,14. Absolute term values are found for the corresponding upper levels C(2,3), D(2,3), and B(10,12,14). Accurate rotational line integrated cross sections have also been obtained for the lines in these bands. Integrated cross sections reported in our earlier papers [J. Chem. Phys. 109, 1751 (1998); 112, 2251 (2000); 115, 3719 (2001); 116, 155 (2002); 117, 10621 (2002); 119, 8373 (2003)] have been revised, and the results reported here comprise the delta(upsilon,0) bands with upsilon=0-3, the epsilon(upsilon,0) bands with upsilon=0-3, the beta(upsilon,0) bands with upsilon=6,7,9-12,14, and the gamma(3,0) band. For each band, the band oscillator strength is obtained from the sum of the line strengths of all rotational lines, and these are compared with other published values. (c) 2006 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ London Imperial Coll Sci & Technol, Blackett Lab, London SW7 2BZ, England. Univ Hong Kong, Dept Chem, Hong Kong, Hong Kong, Peoples R China. Japan Womens Univ, Tokyo 1128681, Japan. RP Yoshino, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kyoshino@cfa.harvard.edu NR 32 TC 5 Z9 5 U1 2 U2 11 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 7 PY 2006 VL 124 IS 5 AR 054323 DI 10.1063/1.2138029 PG 22 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 010FA UT WOS:000235171100041 PM 16468885 ER PT J AU Xiao, YH Novikova, I Phillips, DF Walsworth, RL AF Xiao, YH Novikova, I Phillips, DF Walsworth, RL TI Diffusion-induced Ramsey narrowing SO PHYSICAL REVIEW LETTERS LA English DT Article ID SPECTROSCOPY; COHERENCE; RESONANCE; FRINGES; LINE AB Diffusion-induced Ramsey narrowing is characterized and identified as a general phenomenon, in which diffusion of coherence in and out of an interaction region such as a laser beam induces spectral narrowing of the associated resonance line shape. Illustrative experiments and an intuitive analytical model are presented for this spectral narrowing effect, which occurs commonly in optically interrogated atomic systems and may also be relevant to quantum dots and other solid-state spin systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Xiao, YH (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RI Novikova, Irina/B-9041-2008 NR 19 TC 72 Z9 72 U1 1 U2 17 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 FEB 3 PY 2006 VL 96 IS 4 AR 043601 DI 10.1103/PhysRevLett.96.043601 PG 4 WC Physics, Multidisciplinary SC Physics GA 009AN UT WOS:000235083600028 PM 16486819 ER PT J AU Soejima, A Wen, J AF Soejima, A Wen, J TI Phylogenetic analysis of the grape family (Vitaceae) based on three chloroplast markers SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE atpB-rbcL spacer; chloroplast DNA; rps16 intron; trnL-F; phylogeny; Vitaceae ID ANATOMICAL DEVELOPMENT; FLORAL DEVELOPMENT; PARTHENOCISSUS-INSERTA; VEGETATIVE DEVELOPMENT; VITIS-RIPARIA; NORTH-AMERICA; DNA; INFERENCE; RBCL; SEQUENCES AB Seventy-nine species representing 12 genera of Vitaceae were sequenced for the trnL-F spacer, 37 of which were subsequently sequenced for the atpB-rbcL spacer and the rps16 intron. Phylogenetic analysis of the combined data provided a fairly robust phylogeny for Vitaceae. Cayratia, Tetrastigma, and Cyphostemma form a clade. Cyphostemma and Tetrastigma are each monophyletic, and Cayratia may be paraphyletic. Ampelopsis is paraphyletic with the African Rhoicissus and the South American Cissus striata nested within it. The pinnately leaved Ampelopsis form a subclade, and the simple and palmately leaved Ameplopsis constitutes another with both subclades containing Asian and American species. Species of Cissus from Asia and Central America are monophyletic, but the South American C. striata does not group with other Cissus species. The Asian endemic Nothocissus and Pterisanthes form a clade with Asian Ampelocissus, and A. javalensis from Central America is sister to this clade. Vitis is monophyletic and forms a larger clade with Ampelocissus, Pterisanthes, and Nothocissus. The eastern Asian and North American disjunct Parthenocissus forms a clade with Yua austro-orientalis, a species of a small newly recognized genus from China to eastern Himalaya. Vitaceae show complex multiple intercontinental relationships within the northern hemisphere and between northern and southern hemispheres. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, Washington, DC 20013 USA. Osaka Prefecture Univ, Sch Sci, Dept Biol Sci, Sakai, Osaka 5998531, Japan. Chinese Acad Sci, Inst Bot, Lab Systemat & Evolut Bot, Beijing 100093, Peoples R China. RP Wen, J (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, MRC166, Washington, DC 20013 USA. EM wenj@si.edu NR 74 TC 66 Z9 78 U1 3 U2 10 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 FEB PY 2006 VL 93 IS 2 BP 278 EP 287 DI 10.3732/ajb.93.2.278 PG 10 WC Plant Sciences SC Plant Sciences GA 011UU UT WOS:000235294800012 PM 21646189 ER PT J AU Fonseca, DM Smith, JL Wilkerson, RC Fleischer, RC AF Fonseca, DM Smith, JL Wilkerson, RC Fleischer, RC TI Pathways of expansion and multiple introductions illustrated by large genetic differentiation among worldwide populations of the southern house mosquito SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID LIBERIAN CULEX-QUINQUEFASCIATUS; AVIAN MALARIA; WUCHERERIA-BANCROFTI; MICROSATELLITE LOCI; PIPIENS COMPLEX; NORTH-AMERICA; SUSCEPTIBILITY; VECTOR; HAWAII; CULICIDAE AB The southern house mosquito Cidex quinquefasciatus is a principal vector of human lymphatic filariasis, several encephalitides (including West Nile virus), avian malaria, and poxvirus, but its importance as it vector varies considerably among regions. This species has spread with humans and is ubiquitous in tropical urban and suburban environments. This was the first mosquito to reach Hawaii and we performed a worldwide genetic survey using microsatellite loci to identify its source. Our analyses showed divergent Old World and New World genetic signatures in Cx. quinquefasciatus with further distinctions between cast and west African, Asian, and Pacific populations that correlate with the epidemiology of human filariasis. We found that in Hawaii south Pacific mosquitoes have largely replaced the original New World introduction of Cx. quinquefasciatus, consistent with their reported expansion to higher elevations. We hypothesize worldwide pathways of expansion of this disease vector. C1 Acad Nat Sci Philadelphia, Philadelphia, PA 19103 USA. Smithsonian Inst, Genet Program, Washington, DC 20560 USA. Walter Reed Army Inst Res, Silver Spring, MD USA. RP Fonseca, DM (reprint author), Acad Nat Sci Philadelphia, 1900 Ben Franklin Pkwy, Philadelphia, PA 19103 USA. EM fonseca@acnatsci.org RI Meyer, Julie/D-1021-2010; OI Meyer, Julie/0000-0003-3382-3321; Fonseca, Dina/0000-0003-4726-7100 FU NIGMS NIH HHS [R01GM063258]; PHS HHS [U50/CCU220532] NR 47 TC 42 Z9 45 U1 1 U2 5 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 FEB PY 2006 VL 74 IS 2 BP 284 EP 289 PG 6 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 012OX UT WOS:000235349600019 PM 16474085 ER PT J AU Ekanayake, DK Arulkanthan, A Horadagoda, NU Sanjeevani, GKM Kieft, R Gunatilake, S Dittus, WPJ AF Ekanayake, DK Arulkanthan, A Horadagoda, NU Sanjeevani, GKM Kieft, R Gunatilake, S Dittus, WPJ TI Prevalence of Cryptosporidium and other enteric parasites among wild non-human primates in Polonnaruwa, Sri Lanka SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID GORILLA-GORILLA-BERINGEI; MACAQUES MACACA-SINICA; GASTROINTESTINAL-TRACT PARASITES; TOQUE MACAQUES; INTESTINAL PARASITES; NATURAL-POPULATION; KENYA; TRANSMISSION; INFECTION; HELMINTH AB Cryptosporidiosis is a rapidly emerging disease in the tropics. This is the first report of Cryptosporidium and other protozoan infections (Entamoeba spp., lodamoeba, Chilomastix, and Balantidium Spp.) in wild primates that inhabit the natural forest of Sri Lanka. It is unclear if non-human primates serve as a reservoir for these parasites under certain conditions. A cross-sectional coprologic survey among 125 monkeys (89 toque macaques, 21 gray langurs, and 1.5 purple-faced langurs) indicated that Cryptosporidium was detected in all three primate species and was most common among monkeys using areas and water that had been heavily soiled by human feces and livestock. Most macaques (96%) ;shedding Cryptosporidium oocysts were co-infected with other protozoans and important anthropozoonotic gastrointestinal parasites (e.g., Enterobius and Strongyloides). The transmission of these parasites among primates in the wild may have important implications for public health as well as wildlife conservation management. C1 Assoc Conservat Primate Divers, Kandy, CP, Sri Lanka. Inst Fundamental Studies, Kandy, Sri Lanka. Smithsonian Natl Zool Pk, Dept Environm Conservat, Washington, DC USA. Marine Biol Lab, Global Infect Dis Program, Woods Hole, MA 02543 USA. Univ Peradeniya, Fac Vet Med & Anim Sci, Dept Vet Pathobiol, Peradeniya, Sri Lanka. RP Dittus, WPJ (reprint author), Assoc Conservat Primate Divers, 140-12 Mapanawathura Rd, Kandy, CP, Sri Lanka. EM dittus@sri.lanka.net NR 38 TC 23 Z9 29 U1 0 U2 8 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 FEB PY 2006 VL 74 IS 2 BP 322 EP 329 PG 8 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 012OX UT WOS:000235349600025 PM 16474091 ER PT J AU Warkentin, KM Buckley, CR Metcalf, KA AF Warkentin, KM Buckley, CR Metcalf, KA TI Development of red-eyed treefrog eggs affects efficiency and choices of egg-foraging wasps SO ANIMAL BEHAVIOUR LA English DT Article ID AGALYCHNIS-CALLIDRYAS; PREDATION RISK; HATCHING AGE; DIET; FROG; HYMENOPTERA; ADAPTATIONS; AMPHIBIANS; EVOLUTION; VESPIDAE AB The arboreal eggs of red-eyed treefrogs, Agalychnis callidryas, are preyed on by social wasps, Polybia rejecta. Embryos hatch rapidly up to 30% before their typical undisturbed hatching age when attacked by wasps, so many embryos escape. We hypothesized that the escape ability of older embryos would reduce wasp foraging success or efficiency, and that wasps would therefore prefer to prey on younger eggs. To characterize wasp foraging abilities and preferences, we videotaped the behaviour of individual foragers at an outdoor feeding station. We presented wasps with pairs of clutches differing in age by 1 day, from newly laid versus 1 day through 4 versus 5 days. Eggs become competent to hatch at 4 days. Wasps foraged more efficiently and successfully on older eggs than on younger ones. Among not-yet-patchable clutches, wasps preferred older eggs, but there was no evidence for discrimination between late unhatchable eggs and hatchable eggs (3-5 days), and wasps readily attacked embryos likely to escape. The thick egg jelly of younger clutches makes it difficult for wasps to break into eggs. The poorly developed embryos also disintegrate easily, making them harder to carry. Thus, at least when wasps have experience with a range of egg stages, they kill few young eggs. Older eggs frequently escaped by hatching, so the heaviest mortality fell on intermediate developmental stages, both at the feeding station and at a natural breeding site. Structural variation in egg clutches and developmental changes in embryos may affect interactions between other small, mobile predators and amphibian eggs. (c) 2005 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Boston Univ, Dept Biol, Boston, MA 02215 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM kwarken@bu.edu NR 35 TC 15 Z9 15 U1 0 U2 5 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 FEB PY 2006 VL 71 BP 417 EP 425 DI 10.1016/j.anbehav.2005.06.007 PN 2 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 016OB UT WOS:000235628500018 ER PT J AU Fisk, MR Popa, R Mason, OU Storrie-Lombardi, MC Vicenzi, EP AF Fisk, MR Popa, R Mason, OU Storrie-Lombardi, MC Vicenzi, EP TI Iron-magnesium silicate bioweathering on Earth (and Mars?) SO ASTROBIOLOGY LA English DT Article DE bioweathering; biosignature; olivine; pyroxene; dunite; nakhlite ID AQUEOUS ALTERATION; MICROBIAL ACTIVITY; MARTIAN METEORITE; BASALTIC GLASS; ELECTRON-MICROSCOPY; BIOGENIC ALTERATION; VOLCANIC GLASS; LIFE; BACTERIA; OLIVINE AB We examined the common, iron-magnesium silicate minerals olivine and pyroxene in basalt and in mantle rocks to determine if they exhibit textures similar to bioweathering textures found in glass. Our results show that weathering in olivine may occur as long, narrow tunnels (1-3 mu m in diameter and up to 100 mu m long) and as larger irregular galleries, both of which have distinctive characteristics consistent with biological activity. These weathering textures are associated with clay mineral by-products and nucleic acids. We also examined olivine and pyroxene in martian meteorites, some of which experienced preterrestrial aqueous alteration. Some olivines and pyroxenes in the martian meteorite Nakhla were found to contain tunnels that are similar in size and shape to tunnels in terrestrial iron-magnesium silicates that contain nucleic acids. Though the tunnels found in Nakhla are similar to the biosignatures found in terrestrial minerals, their presence cannot be used to prove that the martian alteration features had a biogenic origin. The abundance and wide distribution of olivine and pyroxene on Earth and in the Solar System make bioweathering features in these minerals potentially important new biosignatures that may play a significant role in evaluating whether life ever existed on Mars. C1 Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Portland State Univ, Dept Biol, Portland, OR 97207 USA. Kinohi Inst, Pasadena, CA USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Fisk, MR (reprint author), Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. EM mfisk@coas.oregonstate.edu NR 90 TC 49 Z9 53 U1 1 U2 15 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD FEB PY 2006 VL 6 IS 1 BP 48 EP 68 DI 10.1089/ast.2006.6.48 PG 21 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 025DR UT WOS:000236246000004 PM 16551226 ER PT J AU Putman, ME Rosenberg, JL Stocke, JT McEntaffer, R AF Putman, ME Rosenberg, JL Stocke, JT McEntaffer, R TI The relationship between baryons and dark matter in extended galaxy halos SO ASTRONOMICAL JOURNAL LA English DT Article DE dark matter; galaxies : halos; galaxies : kinematics and dynamics; galaxies : spiral; intergalactic medium; large-scale structure of universe ID HIGH-VELOCITY CLOUDS; LY-ALPHA FOREST; EXTRA-PLANAR GAS; VIRGO CLUSTER; SPIRAL GALAXIES; DENSITY PROFILE; HI OBSERVATIONS; GALACTIC HALOS; TULLY-FISHER; ABSORBERS AB The relationship between gas-rich galaxies and Ly alpha absorbers is addressed in this paper in the context of the baryonic content of galaxy halos. Deep Arecibo H I observations are presented of two gas-rich spiral galaxies within 125 h(70)(-1) kpc projected distance of a Ly alpha absorber at a similar velocity. The galaxies investigated are close to edge-on, and the absorbers lie almost along their major axes, allowing for a comparison of the Ly alpha absorber velocities with galactic rotation. This comparison is used to examine whether the absorbers are diffuse gas rotating with the galaxies' halos, outflow material from the galaxies, or intergalactic gas in the low-redshift cosmic web. The results indicate that if the gas resides in the galaxies' halos, it is not rotating with the system and is possibly counterrotating. In addition, simple geometry indicates that the gas was not ejected from the galaxies, and there are no gas-rich satellites detected down to 3.6-7.5 x 10(6) M-circle dot or remnants of satellites to 5.6 x 10(18) cm(-2). The gas could potentially be infalling from large radii, but the velocities and distances are rather high compared to the high-velocity clouds around the Milky Way. The most likely explanation is that the galaxies and absorbers are not directly associated, despite the vicinity of the spiral galaxies to the absorbers (58-77 h(70)(-1) kpc from the H I edge). The spiral galaxies reside in a filament of intergalactic gas, and the gas detected by the absorber has not yet come into equilibrium with the galaxy. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Putman, ME (reprint author), Univ Michigan, Dept Astron, 830 Dennison,500 Church St, Ann Arbor, MI 48109 USA. EM mputman@umich.edu; jlrosenberg@cfa.harvard.edu; stocke@colorado.edu NR 60 TC 5 Z9 5 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 FEB PY 2006 VL 131 IS 2 BP 771 EP 781 DI 10.1086/498720 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010RX UT WOS:000235214500009 ER PT J AU Stockdale, CJ Maddox, LA Cowan, JJ Prestwich, A Kilgard, R Immler, S AF Stockdale, CJ Maddox, LA Cowan, JJ Prestwich, A Kilgard, R Immler, S TI A radio and X-ray study of historical supernovae in M83 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual ( M83); radio continuum : galaxies; supernovae : general; supernovae : individual (SN 1923A, SN1945B, SN1950B, SN 1957D, SN 1968L, SN1983N) ID HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC DISTANCE SCALE; RAPID PRESUPERNOVA EVOLUTION; KEY PROJECT; SOURCE POPULATION; LIGHT CURVES; I SUPERNOVA; SN 1978K; NGC 1313; EMISSION AB We report the results of 15 years of radio observations of the six historical supernovae (SNe) in M83 using the Very Large Array. We note the near-linear decline in radio emission from SN 1957D, a Type II SN, which remains a nonthermal radio emitter. The measured flux densities from SNe 1923A and 1950B have flattened as they begin to fade below detectable limits; they are also Type II SNe. The luminosities for these three SNe are comparable with the radio luminosities of other decades-old SNe at similar epochs. SNe 1945B, 1968L, and 1983N were not detected in the most recent observations, and these nondetections are consistent with previous studies. We report the X-ray nondetections of all six historical SNe using the Chandra X-Ray Observatory, consistent with previous X-ray searches of other decades-old SNe and low inferred mass-loss rates of the progenitors [. M approximate to (10(-8) M-circle dot yr(-1)) (nu(w)/10 km s(-1))]. C1 Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Explorat Univ Div, Greenbelt, MD 20771 USA. RP Stockdale, CJ (reprint author), Marquette Univ, Dept Phys, POB 1881, Milwaukee, WI 53201 USA. EM christopher.stockdale@marquette.edu; maddox@nhn.ou.edu; cowan@nhn.ou.edu; aprestwich@cfa.harvard.edu; rkilgard@cfa.harvard.edu; immler@milkyway.gsfc.nasa.gov NR 47 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 FEB PY 2006 VL 131 IS 2 BP 889 EP 894 DI 10.1086/499401 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010RX UT WOS:000235214500019 ER PT J AU Zapata, LA Rodriguez, LF Ho, PTP Beuther, H Zhang, QZ AF Zapata, LA Rodriguez, LF Ho, PTP Beuther, H Zhang, QZ TI In search of circumstellar disks around young massive stars SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : individual (IRAS 18089-1732, IRAS 18182-1433, IRAS 18264-1152, IRAS 18308-0841); radio continuum : ISM; stars : formation; stars : pre-main-sequence ID FORMING REGION; PROTOSTELLAR CANDIDATES; ROTATING-DISK; ACCRETION; SYSTEM; DUST; CONTINUUM; EMISSION; OBJECT; JET AB We present 7 mm, 1.3 cm, and 3.6 cm continuum observations made with the Very Large Array toward a sample of 10 luminous IRAS sources that are believed to be regions of massive star formation. We detect compact 7 mm emission in four of these objects: IRAS 18089-1732(1), IRAS 18182-1433, IRAS 18264-1152, and IRAS 18308-0841, and for the first time find that these IRAS sources are associated with double or triple radio sources separated by a few arcseconds. We discuss the characteristics of these sources based mostly on their spectral indices and find that their natures are diverse. Some features indicate that the 7 mm emission is dominated by dust from disks or envelopes. Toward other components, the 7 mm emission appears to be dominated by free-free radiation, both from ionized outflows or from optically thick H II regions. Furthermore, there is evidence of synchrotron contamination in some of these sources. Finally, we find that the sources associated with ionized outflows or thermal jets are correlated with CH3OH masers. The precise determination of the nature of these objects requires additional multifrequency observations at high angular resolution. The 3.6 cm continuum observations also revealed seven ultracompact (UC) H II regions in the vicinity of the sources IRAS 18089-1732(1), and two more in the source IRAS 18182-1433. We show that the small photoionized nebulae of these UC H II regions are produced by early B-type stars. C1 Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Direcc Gen Asuntos Personal Acad, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Direcc Gen Asuntos Personal Acad, Apartado Postal 3-72, Morelia 58089, Michoacan, Mexico. EM lzapata@astrosmo.unam.mx OI Zhang, Qizhou/0000-0003-2384-6589 NR 37 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2006 VL 131 IS 2 BP 939 EP 950 DI 10.1086/499156 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010RX UT WOS:000235214500023 ER PT J AU Torres, G AF Torres, G TI The astrometric-spectroscopic binary system hip 50796: An overmassive companion SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; binaries : visual; stars : individual ( HIP 50796); stars : late-type; techniques : radial velocities; techniques : spectroscopic ID TW-HYDRAE ASSOCIATION; LOW-MASS STARS; X-RAY; CANDIDATE MEMBERS; RADIAL-VELOCITIES; HYA-ASSOCIATION; HIPPARCOS DATA; PROPER-MOTION; SEARCH AB We report spectroscopic observations of the star HIP 50796, previously considered ( but later rejected) as a candidate member of the TW Hya association. Our measurements reveal it to be a single-lined binary with an orbital period of 570 days and an eccentricity of e = 0.61. The astrometric signature of this orbit was previously detected by Hipparcos in the form of curvature in the proper-motion components, although the period was unknown at the time. By combining our radial velocity measurements with the Hipparcos intermediate data ( abscissa residuals) we are able to derive the full three-dimensional orbit and determine the dynamical mass of the unseen companion, as well as a revised trigonometric parallax that accounts for the orbital motion. Given our primary mass estimate of 0.73 M-circle dot (mid-K dwarf), the companion mass is determined to be 0.89 M-circle dot, or similar to 20% larger than the primary. The likely explanation for the larger mass without any apparent contribution to the light is that the companion is itself a closer binary composed ofMdwarfs. The near-infrared excess and X-ray emission displayed by HIP 50796 support this. Our photometric modeling of the excess leads to a lower limit to the mass ratio of the close binary of q similar to 0.8 and individual masses of 0.44-0.48 and 0.41-0.44 M-circle dot. The new parallax (pi 20: 6 +/- 1.9 mas) is significantly smaller than the original Hipparcos value and more precise. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 34 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2006 VL 131 IS 2 BP 1022 EP 1031 DI 10.1086/498693 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010RX UT WOS:000235214500033 ER PT J AU Skrutskie, MF Cutri, RM Stiening, R Weinberg, MD Schneider, S Carpenter, JM Beichman, C Capps, R Chester, T Elias, J Huchra, J Liebert, J Lonsdale, C Monet, DG Price, S Seitzer, P Jarrett, T Kirkpatrick, JD Gizis, JE Howard, E Evans, T Fowler, J Fullmer, L Hurt, R Light, R Kopan, EL Marsh, KA McCallon, HL Tam, R Van Dyk, S Wheelock, S AF Skrutskie, MF Cutri, RM Stiening, R Weinberg, MD Schneider, S Carpenter, JM Beichman, C Capps, R Chester, T Elias, J Huchra, J Liebert, J Lonsdale, C Monet, DG Price, S Seitzer, P Jarrett, T Kirkpatrick, JD Gizis, JE Howard, E Evans, T Fowler, J Fullmer, L Hurt, R Light, R Kopan, EL Marsh, KA McCallon, HL Tam, R Van Dyk, S Wheelock, S TI The Two Micron All Sky Survey (2MASS) SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; infrared : general; surveys ID CATALOG; CALIBRATION; SYSTEM AB Between 1997 June and 2001 February the Two Micron All Sky Survey (2MASS) collected 25.4 Tbytes of raw imaging data covering 99.998% of the celestial sphere in the near-infrared J ( 1.25 mu m), H(1.65 mu m), and K-s(2.16 mu m) bandpasses. Observations were conducted from two dedicated 1.3 m diameter telescopes located at Mount Hopkins, Arizona, and Cerro Tololo, Chile. The 7.8 s of integration time accumulated for each point on the sky and strict quality control yielded a 10 sigma point-source detection level of better than 15.8, 15.1, and 14.3 mag at the J, H, and Ks bands, respectively, for virtually the entire sky. Bright source extractions have 1 sigma photometric uncertainty of < 0.03 mag and astrometric accuracy of order 100 mas. Calibration offsets between any two points in the sky are < 0.02 mag. The 2MASS All-Sky Data Release includes 4.1 million compressed FITS images covering the entire sky, 471 million source extractions in a Point Source Catalog, and 1.6 million objects identified as extended in an Extended Source Catalog. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. USN Observ, Flagstaff Stn, Flagstaff, AZ 86002 USA. USAF, Res Lab, Bedford, MA 01731 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. OI Weinberg, Martin/0000-0003-2660-2889; Gizis, John/0000-0002-8916-1972; Van Dyk, Schuyler/0000-0001-9038-9950 NR 20 TC 4913 Z9 4938 U1 11 U2 52 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2006 VL 131 IS 2 BP 1163 EP 1183 DI 10.1086/498708 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010RX UT WOS:000235214500046 ER PT J AU Weigelt, G Beuther, H Hoffmann, KH Meyer, MR Preibisch, T Schertl, D Smith, MD Young, ET AF Weigelt, G Beuther, H Hoffmann, KH Meyer, MR Preibisch, T Schertl, D Smith, MD Young, ET TI Bispectrum speckle interferometry of the massive protostellar outflow source IRAS 23151+5912 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : formation ID YOUNG STELLAR OBJECTS; T-TAURI STARS; MOLECULAR OUTFLOWS; H2O MASERS; HYDRODYNAMIC SIMULATIONS; CIRCUMSTELLAR DISKS; HIGH-RESOLUTION; HERBIG; MASKING; JETS AB We present bispectrum speckle interferometry of the massive protostellar object IRAS 23151+5912 in the near-infrared K' band. The reconstructed image shows the diffuse nebulosity north-east of two point-like Sources in unprecedented detail. The comparison Of Our near-infrared image with mm continuum and CO molecular line maps shows that the brighter of the two point Sources lies near the center of the mm peak, indicating that it is a high-mass protostar. The nebulosity coincides with the blue-shifted Molecular outflow component. The most prominent feature in the nebulosity is it bow-shock-like arc. We assume that this feature is associated with a precessing jet which has created an inward-pointed cone in the swept-up material. We present numerical jet simulations that reproduce this and several other features observed in our speckle image of the nebulosity. Our data also reveal a linear structure connecting the central point source to the extended diffuse nebulosity. This feature may represent the innermost part of a jet that drives the strong molecular Outflow (PA similar to 80 degrees) from IRAS 23 151 +5912. With the aid of radiative transfer calculations, we demonstrate that, in general, the observed inner Structures of the circumstellar material surrounding high-mass stars are strongly influenced by the orientation and symmetry of the bipolar cavity. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Armagh Observ, Armagh BT61 9DG, North Ireland. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Weigelt, G (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM preib@mpifr-bonn.mpg.de NR 42 TC 13 Z9 13 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 FEB PY 2006 VL 447 IS 2 BP 655 EP 665 DI 10.1051/0004-6361:20053817 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015IC UT WOS:000235544100030 ER PT J AU Merand, A Borde, P Coude, V du Foresto, VD AF Merand, A Borde, P Coude, V du Foresto, VD TI A catalog of bright calibrator stars for 200-m baseline near-infrared stellar interferometry (vol 433, pg 1155, 2005) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE catalogs; stars : fundamental parameters; techniques : interferometric; instrumentation : interferometers; errata, addenda AB There is labelling mistake in Fig. 1 (Sect. 2), as this plot deals with the non-squared visibility: the correct label for the vertical axis should therefore read delta V/V and the inserted texts should be V > 40% and V < 40%. The revised limit of validity for the uniform disk approximation is then V-2 > 16%. In the body of the article, Sect. 3, another reference is made to this result. The reader should read that the squared visibility limit is V-2 > 16%. The correction of this mistake does not change the main characteristics of the calibrator stars catalog. C1 Observ Paris, LESIA, UMR 8109, F-92195 Meudon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Merand, A (reprint author), Observ Paris, LESIA, UMR 8109, 5 Pl Jules Janssen, F-92195 Meudon, France. EM Antoine.Merand@obspm.fr; pborde@cfa.harvard.edu; Vincent.Foresto@obspm.fr NR 1 TC 14 Z9 14 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 FEB PY 2006 VL 447 IS 2 BP 783 EP 783 DI 10.1051/0004-6361:20041323e PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015IC UT WOS:000235544100042 ER PT J AU Bassa, CG Jonker, PG in 't Zand, JJM Verbunt, F AF Bassa, CG Jonker, PG in 't Zand, JJM Verbunt, F TI Two new candidate ultra-compact X-ray binaries SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : binaries; X-rays : individual : 1A 1246-588, 4U 1812-12 ID 4U-1543-624; 2S-0918-549; PHOTOMETRY; EMISSION; CATALOG; BURSTS; STARS AB We present the identification of the optical counterparts to the low-mass X-ray binaries 1A 1246-588 and 4U 1812-12. We determine the X-ray position of 1A 1246-588 from ROSAT/PSPC observations and find within the error circle a blue star with V = 19.45, B - V = 0.22 and R - I = 0.22 which we identify as the counterpart. Within the Chandra error circle of 4U 1812-12, a single star is present which appears blue with respect to the stars in the vicinity. It has R = 22. 15, R - I = 1.53. Distance estimates for both systems indicate that the optical counterparts are intrinsically faint, suggesting that they are ultra-compact X-ray binaries. These identifications would increase the number of candidate ultra- compact X- ray binaries from 2 to 4, whereas orbital periods are measured for only 7 systems in the Galactic disk. C1 Univ Utrecht, Inst Astron, NL-3508 TA Utrecht, Netherlands. SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bassa, CG (reprint author), Univ Utrecht, Inst Astron, POB 80000, NL-3508 TA Utrecht, Netherlands. EM c.g.bassa@astro.uu.nl NR 26 TC 19 Z9 19 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 FEB PY 2006 VL 446 IS 3 BP L17 EP L20 DI 10.1051/004-6361:200500229 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005CX UT WOS:000234801300001 ER PT J AU Weisskopf, MC Aldcroft, TL Cameron, RA Gandhi, P Foellmi, C Elsner, RF Patel, SK Wu, K O'Dell, SL AF Weisskopf, MC Aldcroft, TL Cameron, RA Gandhi, P Foellmi, C Elsner, RF Patel, SK Wu, K O'Dell, SL TI The first Chandra field SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; history and philosophy of astronomy; X-rays : general ID ACTIVE GALACTIC NUCLEI; EMISSION-LINE PROPERTIES; X-RAY-EMISSION; FE-II EMISSION; BALMER DECREMENT; PG QUASARS; CATACLYSMIC VARIABLES; PHYSICAL CONDITIONS; CORRELATION SPACE; SEYFERT-GALAXIES AB Before the official first- light images, the Chandra X- Ray Observatory obtained an X- ray image of the field to which its focal plane was first exposed. We describe this historic observation and report our study of the first Chandra field. Chandra's Advanced CCD Imaging Spectrometer ( ACIS) detected 15 X- ray sources, the brightest being dubbed Leon X- 1 to honor the Chandra telescope scientist LeonVan Speybroeck. Based on our analysis of the X- ray data and spectroscopy at the European Southern Observatory ( ESO; La Silla, Chile), we find that LeonX- 1 is a type- 1 ( unobscured) active galactic nucleus ( AGN) at redshift z = 0: 3207. Leon X- 1 exhibits strong Fe (II) emission and a broad- line Balmer decrement that is unusually flat for an AGN. Within the context of the eigenvector- 1 correlation space, these properties suggest that Leon X- 1 may be a massive ( >= 10(9) M (circle dot)) black hole, accreting at a rate approaching its Eddington limit. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. European So Observ, Santiago 19, Chile. Univ Space Res Assoc, Huntsville, AL 35805 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP NASA, George C Marshall Space Flight Ctr, NSSTC XD12,3200 Sparkman Dr, Huntsville, AL 35805 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 55 TC 4 Z9 4 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 1 PY 2006 VL 637 IS 2 BP 682 EP 692 DI 10.1086/497907 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600011 ER PT J AU Kassis, M Adams, JD Campbell, MF Deutsch, LK Hora, JL Jackson, JM Tollestrup, EV AF Kassis, M Adams, JD Campbell, MF Deutsch, LK Hora, JL Jackson, JM Tollestrup, EV TI Mid-infrared emission at photodissociation regions in the Orion Nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; HII regions; infrared : ISM; ISM : individual (Orion Nebula) ID POLYCYCLIC AROMATIC-HYDROCARBONS; INFRARED-EMISSION; SUBMILLIMETER OBSERVATIONS; IONIZATION FRONT; BAR; RESOLUTION; OBJECTS; SPECTROMETER; EXTINCTION; MILLIMETER AB The mid-infrared emission from a photodissociation region (PDR) viewed edge-on in the Orion Nebula is examined through 8.7-20.6 mu m images and 8 - 13 mu m spectra. The polycyclic aromatic hydrocarbon (PAH) emission is located between the edges of H II regions and layers of [ C I] emission, agreeing with PDR theory. Using a simple model, the spatial variations in the emission from PAHs detected at 8.6, 11.2, and 12.7 mu m are demonstrated to be directly proportional to the material column density and the intensity of the UV field. For a homogeneous, neutral cloud illuminated by a bright OB star, PDR theory predicts that the ultraviolet ( UV) radiation is attenuated exponentially ( e (-1.8Av)). The predicted UV attenuation is confirmed by observations of broad PAH emission features found at 8.6, 11.2, and 12.7 mu m. The PAH emission is found in cool regions having greater optical depths relative to regions where mid-infrared emission from ionized gas is observed. Through modeling we determine a gas density of 9.7 x 10(4) cm(-3). On large and small size scales, the relative strengths of the 8.6, 11.2, and 12.7 mu m PAH features at the bar of the Orion Nebula indicate that there is not a simple transition from ionized to neutral PAHs across the PDR. C1 Keck Observ, Kamuela, HI 96743 USA. Boston Univ, Dept Astron, Boston, MA 02215 USA. Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, NASA, Infrared Telescope Facil, Hilo, HI 96720 USA. EM mkassis@keck.hawaii.edu OI Hora, Joseph/0000-0002-5599-4650 NR 45 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2006 VL 637 IS 2 BP 823 EP 837 DI 10.1086/498404 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600025 ER PT J AU Keto, E Wood, K AF Keto, E Wood, K TI Observations on the formation of massive stars by accretion SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G10.6-0.4); stars : formation ID H-II REGIONS; ULTRACOMPACT HII REGION; YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; MAIN-SEQUENCE; ROTATING-DISK; HOT CORE; EVOLUTION; G10.6-0.4; EMISSION AB Observations of the H66 alpha recombination line from the ionized gas in the cluster of newly formed massive stars, G10.6-0.4, show that most of the continuum emission derives from the dense gas in an ionized accretion flow that forms an ionized disk or torus around a group of stars in the center of the cluster. The inward motion observed in the accretion flow suggests that despite the equivalent luminosity and ionizing radiation of several O stars, neither radiation pressure nor thermal pressure has reversed the accretion flow. The observations indicate why the radiation pressure of the stars and the thermal pressure of the H II region are not effective in reversing the accretion flow. The observed rate of the accretion flow, 10(-3) M-circle dot yr(-1), is sufficient to form massive stars within the timescale imposed by their short main-sequence lifetimes. A simple model of disk accretion relates quenched H II regions, trapped hyper-compact H II regions, and photoevaporating disks in an evolutionary sequence. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 66 TC 72 Z9 72 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 1 PY 2006 VL 637 IS 2 BP 850 EP 859 DI 10.1086/498611 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600027 ER PT J AU Walsh, AJ Bourke, TL Myers, PC AF Walsh, AJ Bourke, TL Myers, PC TI Observations of global and local infall in NGC 1333 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : kinematics and dynamics; stars : formation ID YOUNG STELLAR CLUSTERS; STAR-FORMATION; PROTOSTELLAR COLLAPSE; PHYSICAL CONDITIONS; RADIATIVE-TRANSFER; MOLECULAR LINE; SERPENS SMM4; DENSE GAS; MOTIONS; CORES AB We report "infall asymmetry'' in the HCO+(1-0) and (3-2) lines toward NGC 1333, extended over similar to 0.39 pc(2), a larger extent than has been reported before for any star-forming region. The infall asymmetry extends over a major portion of the star-forming complex, and is not limited to a single protostar, a single dense core, or a single spectral line. It seems likely that the infall asymmetry represents inward motions, and that these motions are physically associated with the complex. Both blue-asymmetric and red-asymmetric lines are seen, but in both the (3-2) and (1-0) lines of HCO+ the vast majority of the asymmetric lines are blue, indicating inward motions. The (3-2) line, tracing denser gas, has the spectra with the strongest asymmetry; these spectra are associated with the protostars IRAS 4A and 4B, which most likely indicates that a warm central source is affecting the line profiles. The (3-2) and ( 1-0) lines usually have the same sense of asymmetry in common positions, but their profiles differ significantly, and the (1-0) line appears to trace motions on much larger spatial scales than does the ( 3-2) line. Line profile models fit the spectra well, but do not strongly constrain their parameters. The mass accretion rate of the inward motions is of order 10(-4) M-circle dot yr(-1), similar to the ratio of stellar mass to cluster age. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. EM awalsh@cfa.harvard.edu RI Walsh, Andrew/B-5627-2013 OI Walsh, Andrew/0000-0001-9506-0855 NR 36 TC 19 Z9 19 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 1 PY 2006 VL 637 IS 2 BP 860 EP 868 DI 10.1086/498564 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600028 ER PT J AU Remillard, RA McClintock, JE Orosz, JA Levine, AM AF Remillard, RA McClintock, JE Orosz, JA Levine, AM TI The X-ray outburst of H1743-322 in 2003: High-frequency QPOs with a 3 : 2 frequency ratio SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; relativity; stars : individual ( H1743-322); stars : oscillations; X-rays : binaries ID QUASI-PERIODIC OSCILLATIONS; MICROQUASAR GRO J1655-40; XTE J1550-564; RXTE OBSERVATIONS; DISCOVERY; RESONANCE; BEHAVIOR; MODEL; X-1 AB The 2003 X- ray outburst of the candidate black hole binary, H1743 - 322, was investigated in frequent pointed observations ( 2 - 250 keV) with the Rossi X- Ray Timing Explorer ( RXTE). One particular program of 130 observations is organized into 111 time intervals and searched for the presence of high- frequency quasi- periodic oscillations ( HFQPOs) in the range 50 - 2000 Hz. Only a single observation ( 2003 June 13) yields a detection above 4 sigma. The central frequency of 239 +/- 4 Hz is consistent with the 240 Hz QPO reported for this source on 2003 May 28 ( Homan and coworkers). We group the observations in several different ways and compute average power- density spectra ( PDS) in a search for further evidence of HFQPOs. Significant results are found for two groups defined by the presence of low- frequency QPOs ( 0.1 - 20 Hz) and an absence of " band- limited'' power continua. ( 1) The nine time intervals with the highest X- ray flux yield a QPO at 166 +/- 5 Hz. ( 4.1 sigma; 3 - 35 keV). ( 2) The group with lower X- ray flux ( 24 time intervals) produces a QPO at 242 +/- 3 Hz ( 6.0 sigma; 7 - 35 keV). The ratio of these two frequencies is 1: 46 +/- 0: 05. This finding is consistent with results obtained for three other black hole systems that exhibit commensurate HFQPOs in a 3: 2 ratio. Furthermore, the occurrence of H1743 - 322' s slower HFQPO at times of higher X- ray luminosity closely resembles the behavior of XTE J1550 - 564 and GRO J1655 - 40. We discuss our results in terms of resonance models that invoke frequencies set by general relativity. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM rr@space.mit.edu; jem@cfa.harvard.edu; orosz@sciences.sdsu.edu; aml@space.mit.edu NR 42 TC 27 Z9 27 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 FEB 1 PY 2006 VL 637 IS 2 BP 1002 EP 1009 DI 10.1086/498556 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600041 ER PT J AU Fischer, DA Laughlin, G Marcy, GW Butler, RP Vogt, SS Johnson, JA Henry, GW McCarthy, C Ammons, M Robinson, S Strader, J Valenti, JA McCullough, PR Charbonneau, D Haislip, J Knutson, HA Reichart, DE McGee, P Monard, B Wright, JT Ida, S Sato, B Minniti, D AF Fischer, DA Laughlin, G Marcy, GW Butler, RP Vogt, SS Johnson, JA Henry, GW McCarthy, C Ammons, M Robinson, S Strader, J Valenti, JA McCullough, PR Charbonneau, D Haislip, J Knutson, HA Reichart, DE McGee, P Monard, B Wright, JT Ida, S Sato, B Minniti, D TI The N2K consortium. III. Short-period planets orbiting HD 149143 and HD 109749 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (HD 149143, HD 109749) ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR PLANETS; GALACTIC DISK; GIANT PLANETS; 2001 CAMPAIGN; HOT SATURN; SEARCH; STARS; MODELS AB We report the detection of two short-period planets discovered at Keck Observatory. HD 149143 is a metal-rich G0 IV star with a planet of M sin i = 1.33 M-J and an orbital radius of 0.053 AU. The best-fit Keplerian model has an orbital period, P = 4.072 days, semivelocity amplitude, K = 149.6 m s(-1), and eccentricity, e = 0.016 +/- 0.01. The host star is chromospherically inactive and metal-rich, with [Fe/H] = 0.26. Based on the TeA and stellar luminosity, we derive a stellar radius of 1.49 R-circle dot. Photometric observations of HD 149143 were carried out using the automated photometric telescopes at Fairborn Observatory. HD 149143 is photometrically constant over the radial velocity period to 0.0003 +/- 0.0002 mag, supporting the existence of the planetary companion. No transits were detected down to a photometric limit of approximately 0.02%, eliminating transiting planets with a variety of compositions and constraining the orbital inclination to less than 83 degrees. A short-period planet was also detected around HD 109749, a G3 IV star. HD 109749 is chromospherically inactive, with [Fe/H] = 0.25 and a stellar radius of 1.24. The radial velocities for HD 109749 are modeled by a Keplerian with P = 5.24 days and K = 28.7 m s(-1). The inferred planet mass is M sin i = 0.28 M-J and the semimajor axis of this orbit is 0.0635 AU. Photometry of HD 109749 was obtained with the SMARTS consortium telescope, the PROMPT telescope, and by transitsearch.org observers in Adelaide and Pretoria. These observations did not detect a decrement in the brightness of the host star at the predicted ephemeris time, and they constrain the orbital inclination to less than 85 degrees for gas giant planets with radii down to 0.7R(J). C1 San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA. Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. Bronberg Observ, ZA-0157 Pretoria, South Africa. Tokyo Inst Technol, Meguro Ku, Tokyo 1528551, Japan. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Kobe Univ, Grad Sch Sci & Technol, Kobe, Hyogo 6578501, Japan. Pontificia Univ Catolica, Dept Astron, Santiago 200, Chile. RP San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. EM fischer@stars.sfsu.edu RI Butler, Robert/B-1125-2009; Ida, Shigeru/A-7840-2014; OI Ida, Shigeru/0000-0002-9676-3891; Charbonneau, David/0000-0002-9003-484X; Wright, Jason/0000-0001-6160-5888; Fischer, Debra/0000-0003-2221-0861 NR 46 TC 24 Z9 24 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 1 PY 2006 VL 637 IS 2 BP 1094 EP 1101 DI 10.1086/498557 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600048 ER PT J AU Vrtilek, SD Penninx, W Raymond, JC Verbunt, F Hertz, P Wood, K Lewin, WHG Mitsuda, K AF Vrtilek, SD Penninx, W Raymond, JC Verbunt, F Hertz, P Wood, K Lewin, WHG Mitsuda, K TI Observations of scorpius X-1 with IUE: Ultraviolet results from a multiwavelength campaign (vol 376, pg 278, 1991) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TC Utrecht, Netherlands. USN, Res Lab, Washington, DC 20375 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 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 FEB 1 PY 2006 VL 637 IS 2 BP 1148 EP 1148 DI 10.1086/498411 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000235131600054 ER PT J AU Sun, M Jones, C Forman, W Nulsen, PEJ Donahue, M Voit, GM AF Sun, M Jones, C Forman, W Nulsen, PEJ Donahue, M Voit, GM TI A 70 kiloparsec X-ray tail in the cluster A3627 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : clusters : individual (A3627) galaxies : individual (ESO 137-001); X-rays : galaxies ID MASSIVE GALAXY CLUSTER; LARGE-SCALE STRUCTURES; MILKY-WAY; VIRGO CLUSTER; ABELL 3627; GAS; NEARBY; EVOLUTION; A1367 AB We present the discovery of a 70 kpc X-ray tail behind the small late-type galaxy ESO 137-001, in the nearby, hot (T=6.5 keV) merging cluster A3627, from both Chandra and XMM-Newton observations. The tail has a length-to-width ratio of similar to 10. It is luminous (L0.5-2 keV similar to 10(41) ergs s(-1)), with a temperature of similar to 0.7 keV and an X-ray M-gas of similar to 10(9) M-circle dot (similar to 10% of the galaxy's stellar mass). We interpret this tail as the stripped interstellar medium of ESO 137-001 mixed with the hot cluster medium, with this blue galaxy being converted into a gas-poor galaxy. Three X-ray point sources are detected in the axis of the tail, which may imply active star formation there. The straightness and narrowness of the tail also imply that the turbulence in the intracluster medium is not strong on scales of 20-70 kpc. C1 Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM sunm@pa.msu.edu RI Donahue, Megan/B-5361-2012; OI Voit, Gerard/0000-0002-3514-0383 NR 23 TC 43 Z9 43 U1 0 U2 1 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 1 PY 2006 VL 637 IS 2 BP L81 EP L84 DI 10.1086/500590 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SD UT WOS:000235131900004 ER PT J AU Henry, JP Mullis, CR Voges, W Bohringer, H Briel, UG Gioia, IM Hochra, JP AF Henry, JP Mullis, CR Voges, W Bohringer, H Briel, UG Gioia, IM Hochra, JP TI The ROSAT north ecliptic pole survey: The X-ray catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : active; galaxies : clusters : general; surveys; X-rays : galaxies : clusters; X-rays : general; X-rays : stars ID BRIGHTEST CLUSTER SAMPLE; ALL-SKY SURVEY; EVOLUTION; GALAXIES; OBJECTS AB The sky around the north ecliptic pole (NEP), at alpha(J2000.0) 18(h)00(m)00(s), delta(J2000.0) = +66 degrees 33'39", has the deepest exposure of the entire ROSAT All-Sky Survey (RASS). The NEP is an undistinguished region of moderate Galactic latitude, b = 29.degrees 8, and hence suitable for compiling statistical samples of both Galactic and extragalactic objects. We have made such a compilation in the 80.6 deg(2) region surrounding the NEP. Our sample fully exploits the properties of the RASS, since the only criteria for inclusion are source position and significance, and it yields the deepest large solid angle contiguous sample of X-ray sources to date. We find 442 unique sources above a flux limit similar to 2; 10(-14) ergs cm(-2) s(-1) in the 0.5-2.0 keV band. In this paper we present the X-ray properties of these sources as determined from the RASS. These include positions, fluxes, spectral information in the form of hardness ratios, and angular sizes. Since we have performed a comprehensive optical identification program we also present the average X-ray properties of classes of objects typical of the X-ray sky at these flux levels. We discuss the use of the RASS to find clusters of galaxies based on their X-ray properties alone. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CNR, Ist Radioastron INAF, I-40129 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Salem, MA 01970 USA. RP Henry, JP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM henry@ifa.hawaii.edu RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 32 TC 38 Z9 38 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 FEB PY 2006 VL 162 IS 2 BP 304 EP 328 DI 10.1086/498749 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013QW UT WOS:000235425300002 ER PT J AU Buckalew, BA Kobulnicky, HA Darnel, JM Polomski, E Gehrz, RD Humphreys, RM Woodward, CE Hinz, JL Engelbracht, CW Gordon, KD Misselt, K Perez-Gonzalez, PG Rieke, GH Willner, SP Ashby, ML Barmby, P Pahre, MA Roellig, TL Devereux, N Loon, JT Brandl, B AF Buckalew, BA Kobulnicky, HA Darnel, JM Polomski, E Gehrz, RD Humphreys, RM Woodward, CE Hinz, JL Engelbracht, CW Gordon, KD Misselt, K Perez-Gonzalez, PG Rieke, GH Willner, SP Ashby, ML Barmby, P Pahre, MA Roellig, TL Devereux, N Loon, JT Brandl, B TI Understanding radio-selected thermal sources in M33: Ultraviolet, optical, near-infrared, spitzer mid-infrared, and radio observations SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE dust, extinction; galaxies : individual (M33); galaxies : star clusters; infrared : ISM; ISM : structure ID WOLF-RAYET STARS; SUPERNOVA-REMNANTS; GALAXIES; SAMPLE; CLUSTERS; EMISSION; REGIONS; GAS AB We present ultraviolet, optical, near-infrared, Spitzer mid-infrared, and radio images of 14 radio-selected objects in M33. These objects are thought to represent the youngest phase of star cluster formation. We have detected the majority of cluster candidates in M33 at all wavelengths. From the near-IR images, we derived ages 2-10 Myr, K-S-band extinctions (A(Ks)) of 0-1 mag, and stellar masses of 10(3)-10(4) M.. We have generated spectral energy distributions (SEDs) of each cluster from 0.1 to 160 mu m. From these SEDs, we have modeled the dust emission around these star clusters to determine the dust masses (1-10(3) M.) and temperatures (40-90 K) of the clusters' local interstellar medium. Extinctions derived from the JHK(S), H alpha, and UV images are similar to within a factor of 2 or 3. These results suggest that 11 of the 14 radio-selected objects are optically visible young star clusters with a surrounding H II region, that 2 are background objects, possibly active galactic nuclei (AGNs), and that 1 is a Wolf-Rayet star with a surrounding H II region. C1 Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Embry Riddle Aeronaut Univ, Dept Phys, Prescott, AZ 86301 USA. Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Buckalew, BA (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. EM mrk1236@uwyo.edu; chipk@uwyo.edu; jdarnel@uwyo.edu; gehrz@astro.umn.edu; roberta@astro.umn.edu; chelsea@astro.umn.edu; jhinz@as.arizona.edu; cengelbracht@as.arizona.edu; kgordon@as.arizona.edu; kmisselt@as.arizona.edu; pgperez@as.arizona.edu; grieke@as.arizona.edu; swillner@cfa.harvard.edu; mashby@cfa.harvard.edu; pbarmby@cfa.harvard.edu; mpahre@cfa.harvard.edu; thomas.l.roellig@nasa.gov; devereux@erau.edu; jacco@astro.keele.ac.uk; brandl@isc.astro.cornell.edu RI Barmby, Pauline/I-7194-2016; Perez-Gonzalez, Pablo/J-2871-2016 OI Barmby, Pauline/0000-0003-2767-0090; Perez-Gonzalez, Pablo/0000-0003-4528-5639 NR 21 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 FEB PY 2006 VL 162 IS 2 BP 329 EP 345 DI 10.1086/498572 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 013QW UT WOS:000235425300003 ER PT J AU Li, XY Meixner, T Sickman, JO Miller, AE Schimel, JP Melack, JM AF Li, XY Meixner, T Sickman, JO Miller, AE Schimel, JP Melack, JM TI Decadal-scale dynamics of water, carbon and nitrogen in a California chaparral ecosystem: DAYCENT modeling results SO BIOGEOCHEMISTRY LA English DT Article DE carbon and nitrogen cycling; chaparral ecosystem; DAYCENT; drying-rewetting pulse; fire disturbance; Mediterranean-climate; nitrogen deposition ID SAN-BERNARDINO MOUNTAINS; DRYING-REWETTING FREQUENCY; WESTERN UNITED-STATES; INDUCED AGE GRADIENT; SOUTHERN-CALIFORNIA; ADENOSTOMA-FASCICULATUM; CEANOTHUS-MEGACARPUS; SEED-GERMINATION; SIERRA-NEVADA; SOIL CARBON AB The Mediterranean climate, with its characteristic of dry summers and wet winters, influences the hydrologic and microbial processes that control carbon ( C) and nitrogen (N) biogeochemical processes in chaparral ecosystems. These biogeochemical processes in turn determine N cycling under chronic N deposition. In order to examine connections between climate and N dynamics, we quantified decadal-scale water, C and N states and fluxes at annual, monthly and daily time steps for a California chaparral ecosystem in the Sierra Nevada using the DAYCENT model. The daily output simulations of net mineralization, stream flow and stream nitrate (NO3-) export were developed for DAYCENT in order to simulate the N dynamics most appropriate for the abrupt rewetting events characteristic of Mediterranean chaparral ecosystems. Overall, the magnitude of annual modeled net N mineralization, soil and plant biomass C and N, nitrate export and gaseous N emission agreed with those of observations. Gaseous N emission was a major N loss pathway in chaparral ecosystems, in which nitric oxide ( NO) is the dominant species. The modeled C and N fluxes of net primary production (NPP), N uptake and N mineralization, NO3- export and gaseous N emission showed both high inter-annual and intraannual variability. Our simulations also showed dramatic fire effects on NPP, N uptake, N mineralization and gaseous N emission for three years of post. re. The decease in simulated soil organic C and N storages was not dramatic, but lasted a longer time. For the seasonal pattern, the predicted C and N. uxes were greatest during December to March, and lowest in the summer. The model predictions suggested that an increase in the N deposition rate would increase N losses through gaseous N emission and stream N export in the chaparral ecosystems of the Sierra Nevada due to changes in N saturation status. The model predictions could not capture stream NO3- export during most rewetting events suggesting that a dry-rewetting mechanism representing the increase in N mineralization following soil wetting needs to be incorporated into biogeochemical models of semi-arid ecosystems. C1 Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Florida, Inst Food & Agr Sci, Dept Soil & Water Sci, Gainesville, FL 32611 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. RP Li, XY (reprint author), Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. EM lix@si.edu NR 53 TC 32 Z9 33 U1 4 U2 44 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD FEB PY 2006 VL 77 IS 2 BP 217 EP 245 DI 10.1007/s10533-005-1391-z PG 29 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 013ZW UT WOS:000235449500005 ER PT J AU Schulze, A AF Schulze, A TI Phylogeny and genetic diversity of palolo worms (Palola, Eunicidae) from the tropical North Pacific and the Caribbean SO BIOLOGICAL BULLETIN LA English DT Article ID POLYCHAETA-ANNELIDA; VIRIDIS POLYCHAETA; MITOCHONDRIAL-DNA; SEQUENCES; REPRODUCTION; SICILIENSIS; EPITOKY; MODELS; SAMOA; GRAY AB Palolo worms (Palola, Eunicidae) are best known for their annual mass spawnings, or "risings," in the South Pacific. Palola currently contains 14 morphologically similar species, mostly from shallow tropical waters. In this study, 60 specimens of Palola from nine locations in the tropical North Pacific and the Caribbean were sequenced for the two mitochondrial markers cytochrome c oxidase subunit I and 16S ribosomal RNA to infer phylogenetic relationships, genetic diversity, and phylogeography within the taxon. Phylogenetic analysis was performed using Bayesian statistics and parsimony. Vouchers of the same specimens were examined morphologically. Two major clades (A and B) can be distinguished within the monophyletic Palola. A number of individuals in clade B bear rows of ventral eyespots in the posterior body region, typical for swarming P. viridis and probably a synapomorphy for clade B. No morphological synapomorphy was found for clade A. Haplotypes from divergent clades often co-occur in the same location. Some haplotypes are geographically widespread, in one case covering the entire east-west expansion of the tropical Pacific. These result simply that despite the apparent absence of teleplanic larvae in eunicid polychaetes, long-distance dispersal is possible in at least some lineages of Palola. C1 Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Schulze, A (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM schulze@sms.si.edu RI Schulze, Anja/I-4215-2012 NR 64 TC 22 Z9 24 U1 1 U2 37 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD FEB PY 2006 VL 210 IS 1 BP 25 EP 37 DI 10.2307/4134534 PG 13 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 020OK UT WOS:000235919000004 PM 16501062 ER PT J AU Agnarsson, I AF Agnarsson, I TI Asymmetric female genitalia and other remarkable morphology in a new genus of cobweb spiders (Theridiidae, Araneae) from Madagascar SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE antisymmetry; asymmetric epigyna; clypeal proboscis; copulation; mating; Pholcommatinae; prosomal pits; stridulation; theridiid phylogeny ID ARGYRODES THERIDIIDAE; CLYPEAL GLAND; PHYLOGENY; ANELOSIMUS; ARACHNIDA; DIVERSITY; PHOLCIDAE; LIMITS AB Symmetry is such a conspicuous feature of life that asymmetries draw our immediate attention. While not uncommon in bilateral organisms in general, asymmetry in spiders is rare. Here I report the first case of antisymmetry in external female genitalia in spiders, in the new genus Asygyna (Theridiidae: Araneae) from Madagascar. In the nearly 39 000 species of spiders described to date, the external structure of the female genitalia is symmetric. In entelegyne spiders paired external copulatory openings each lead to an internal copulatory duct, whose roughly symmetrical trajectories terminate in paired receptacles, the spermathecae. In Asygyna, here exemplified by two new species, A. huberi and A. coddingtoni, laterality is evident in the internal and external female genitalia. A single copulatory opening leads (either to the left or right depending on the individual) to a single copulatory duct with a distinctly asymmetric trajectory. The duct splits terminally shortly before entering the two spermathecae. The males are symmetric, but possibly only one palp can be used in copulation with each female. If adaptive, the selective forces behind this asymmetry are perplexing, as male access to females seems reduced. However, if males are plentiful, asymmetry may benefit the female by reducing insertion times and thus shortening copulation time, and by tightening her control over which males sire her offspring. Asygyna has a range of other bizarre sex-related morphologies, including prosomal pits and a well developed stridulatory mechanism in both sexes, a male proboscis, and simplified palps. A phylogenetic analysis, including 63 taxa and 242 morphological characters, places Asygyna in Pholcommatinae, sister to the enigmatic genus Carniella. (c) 2006 The Linnean Society of London, Biological Journal of the Linnean Society, 2006, 87, 211-232. C1 Smithsonian Inst, Washington, DC 20013 USA. Univ British Columbia, Dept Bot & Zool, Vancouver, BC V6T 1Z4, Canada. RP Agnarsson, I (reprint author), Smithsonian Inst, E-530,NHB-105,POB 37012, Washington, DC 20013 USA. EM ingi@zoology.ubc.ca NR 60 TC 17 Z9 18 U1 1 U2 7 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 FEB PY 2006 VL 87 IS 2 BP 211 EP 232 DI 10.1111/j.1095-8312.2006.00569.x PG 22 WC Evolutionary Biology SC Evolutionary Biology GA 006SY UT WOS:000234918800004 ER PT J AU Camargo, A De Sa, RO Heyer, WR AF Camargo, A De Sa, RO Heyer, WR TI Phylogenetic analyses of mtDNA sequences reveal three cryptic lineages in the widespread neotropical frog Leptodactylus fuscus (Schneider, 1799) (Anura, Leptodactylidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Amphibia; cryptic speciation; phylogeography; South America; species concept; species delimitation ID ADVERTISEMENT CALL VARIATION; BUFO MICROSCAPHUS COMPLEX; MITOCHONDRIAL-GENE TREES; EREMICUS SPECIES GROUP; 12S RIBOSOMAL-RNA; MOLECULAR SYSTEMATICS; GEOGRAPHICAL-DISTRIBUTION; INFERRING PHYLOGENIES; DEVELOPMENTAL ARREST; SECONDARY STRUCTURE AB Leptodactylus fuscus is a neotropical frog ranging from Panama to Argentina, to the east of the Andes mountains, and also inhabiting Margarita, Trinidad, and the Tobago islands. We performed phylogenetic analyses of 12S rRNA, 16S rRNA, tRNA-Leu, and ND1 mitochondrial (mt) DNA sequences from specimens collected across the geographic distribution of L. fuscus to examine two alternative hypotheses: (i) L. fuscus is a single, widely distributed species, or (ii) L. fuscus is a species complex. We tested statistically for geographic association and partitioning of genetic variation among mtDNA clades. The mtDNA data supported the hypothesis of several cryptic species within L. fuscus. Unlinked mtDNA and nuclear markers supported independently the distinctness of a 'northern' phylogenetic unit. In addition, the mtDNA data divided the southern populations into two clades that showed no sister relationship to each other, consistent with high differentiation and lack of gene flow among southern populations as suggested by allozyme data. Concordance between mtDNA and allozyme patterns suggests that cryptic speciation has occurred in L. fuscus without morphological or call differentiation. This study illustrates a case in which lineage splitting during the speciation process took place without divergence in reproductive isolation mechanisms (e.g. advertisement call in frogs), contrary to expectations predicted using a biological species framework. (c) 2006 The Linnean Society of London, Biological Journal of the Linnean Society, 2006, 87, 325-341. No claim to original US government works. C1 Univ Richmond, Dept Biol, Richmond, VA 23173 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Camargo, A (reprint author), Fac Ciencias, Secc Zool Vertebrados, 4225 Igua, Montevideo 11400, Uruguay. EM arley@fcien.edu.uy RI Camargo Bentaberry, Arley/A-2975-2008 OI Camargo Bentaberry, Arley/0000-0001-7734-8679 NR 78 TC 40 Z9 44 U1 2 U2 16 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 FEB PY 2006 VL 87 IS 2 BP 325 EP 341 DI 10.1111/j.1095-8312.2006.00581.x PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 006SY UT WOS:000234918800011 ER PT J AU Ewers, RM Didham, RK AF Ewers, RM Didham, RK TI Confounding factors in the detection of species responses to habitat fragmentation SO BIOLOGICAL REVIEWS LA English DT Review DE area effects; edge effects; habitat fragmentation; habitat loss; invertebrate; isolation; matrix; shape index; synergies; time lags ID AMAZONIAN FOREST FRAGMENTS; WING-DIMORPHIC INSECT; RANDOM SAMPLE HYPOTHESIS; EXTINCTION RISK; RAIN-FOREST; FLUCTUATING ASYMMETRY; LANDSCAPE STRUCTURE; METAPOPULATION DYNAMICS; PATCH SHAPE; COMMUNITY STRUCTURE AB Habitat loss has pervasive and disruptive impacts on biodiversity in habitat remnants. The magnitude of the ecological impacts of habitat loss can be exacerbated by the spatial arrangement - or fragmentation - of remaining habitat. Fragmentation per se is a landscape-level phenomenon in which species that survive in habitat remnants are confronted with a modified environment of reduced area, increased isolation and novel ecological boundaries. The implications of this for individual organisms are many and varied, because species with differing life history strategies are differentially affects by habitat fragmentation. Here, we review the extensive literature on species responses to habitat fragmentation, and detail the numerous ways in which confounding factors have either masked the detection, or prevented the manifestation, of predicted fragmentation effects. Large numbers of empirical studies continue to document changes in species richness with decreasing habitat area, wit positive, negative and no relationships regularly reported. The debate surrounding such widely contrasting results is beginning to be resolved by findings that the expected positive species-area relationship can be masked by matrix-derived spatial subsides of resources to fragment-swelling species and by invasion of matrix-dwelling species into habitat edges. Significant advances have been made recently in our understanding of how species interactions are altered at habitat edges as a result of these changes. Interestingly, changes in biotic and abiotic parameters at edges also make ecological processes more variable than in habitat interiors. Individuals are more likely to encounter habitat edges in fragments wit convoluted shapes, leading to increased turnover and variability in population size that in fragments that are compact in shape. Habitat isolation in both space and time disrupts species distribution patterns, with consequent effects on metapopulation dynamics and the genetic structure of fragment-dwelling populations. Again, the matrix habitat is a strong determinant of fragmentation effects within remnants because of its role in regulating dispersal and dispersal-related mortality, the provision of spatial subsides and the potential mediation of edge-related microclimatic gradients. We show that confounding factors can mask many fragmentation effects. For instance, there are multiple ways in which species traits like trophic level, dispersal ability and degree of habitat specialisation influence species-level responses. The temporal scale of investigation may have a Strong influence Oil the results Ora study, with short-term crowding effects eventually giving way to long-term extinction debts. Moreover. many fragmentation effects like changes in genetic, morphological or behavioural traits Of Species require time to appear. By contrast, synergistic interactions of fragmentation with climate change, human-altered disturbance regimes, species interactions and other drivers of population decline may magnify the impacts of fragmentation. To conclude, we emphasise that anthropogenic fragmentation is a recent phenomenon in evolutionary time and suggest that the final, long-term impacts of habitat fragmentation may not yet have shown themselves. C1 Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand. Smithsonian Trop Res Inst, Balboa, Panama. RP Ewers, RM (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM raphael.didham@canterbury.ac.nz RI Didham, Raphael/B-5953-2011; Wrbka, Thomas/A-5699-2010 OI Wrbka, Thomas/0000-0002-1451-9108 NR 310 TC 804 Z9 837 U1 87 U2 773 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 1464-7931 J9 BIOL REV JI Biol. Rev. PD FEB PY 2006 VL 81 IS 1 BP 117 EP 142 DI 10.1017/S1464793105006949 PG 26 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 023CA UT WOS:000236101600005 PM 16318651 ER PT J AU Hagedorn, M Pan, R Cox, EF Hollingsworth, L Krupp, D Lewis, TD Leong, JC Mazur, P Rall, WF MacFarlane, DR Fahy, G Kleinhans, FW AF Hagedorn, M Pan, R Cox, EF Hollingsworth, L Krupp, D Lewis, TD Leong, JC Mazur, P Rall, WF MacFarlane, DR Fahy, G Kleinhans, FW TI Coral larvae conservation: Physiology and reproduction SO CRYOBIOLOGY LA English DT Article DE membrane permeability; larval settlement; chill sensitivity; glycerol ID CRASSOSTREA-GIGAS EMBRYOS; DANIO-RERIO EMBRYOS; BRACHYDANIO-RERIO; CHILLING INJURY; ZEBRAFISH EMBRYOS; STARFISH OOCYTES; FUNGIA-SCUTARIA; PACIFIC OYSTER; PLANULA LARVAE; CLIMATE-CHANGE AB Coral species throughout the world's oceans are facing severe environmental pressures. We are interested in conserving coral larvae by means of cryopreservation, but little is known about their cellular physiology or cryobiology. These experiments examined cryoprotectant toxicity, dry weight, water and cryoprotectant permeability using cold and radiolabeled glycerol, spontaneous ice nucleation temperatures, chilling sensitivity, and settlement of coral larvae. Our two test species of coral larvae, Pocillopora damicornis (lace coral), and Fungia scutaria (mushroom coral) demonstrated a wide tolerance to cryoprotectants. Computer-aided morphometry determined that F scutaria larvae were smaller than P. damicornis larvae. The average dry weight for P. damicornis was 24.5%, while that for F scutaria was 17%, yielding osmotically inactive volumes (V-b) of 0.22 and 0.15, respectively. The larvae from both species demonstrated radiolabeled glycerol uptake over time, suggesting they were permeable to the glycerol. Parameter fitting of the F scutaria larvae data yielded a water permeability >= 2 mu m/min/atm and a cryoprotectant permeability = 2.3 x 10(-4) cm/min while modeling indicated that glycerol reached 90% of final concentration in the larvae within 25 min. The spontaneous ice nucleation temperature for F. scutaria larvae in filtered seawater was -37.8 +/- 1.4 degrees C. However, when E scutaria larvae were chilled from room temperature to -11 degrees C at various rates, they exhibited 100% mortality. When instantly cooled from room temperature to test temperatures, they showed damage below 10 degrees C. These data suggest that the,,, are sensitive to both the rate of chilling and the absolute temperature, and indicate that vitrification may be the only means to successfully cryopreserve these organisms. Without prior cryopreservation, both species of coral settled under laboratory conditions. (C) 2005 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. Univ Tennessee, Dept Biochem & Mol Cellular Biol, Knoxville, TN 37996 USA. NIH, Div Vet Resources, Off Res Serv, Bethesda, MD 20892 USA. Monash Univ, Sch Chem, Clayton, Vic 3168, Australia. 21st Century Med Inc, Cucamonga, CA 91730 USA. Indiana Univ Purdue Univ, Dept Phys, Indianapolis, IN 46202 USA. RP Hagedorn, M (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. EM hagedornm@si.edu RI Rall, William/C-5104-2008; MacFarlane, Douglas/A-9642-2008 OI MacFarlane, Douglas/0000-0001-5963-9659 FU NCRR NIH HHS [RR-16467] NR 52 TC 23 Z9 26 U1 2 U2 22 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 FEB PY 2006 VL 52 IS 1 BP 33 EP 47 DI 10.1016/j.cryobiol.2005.09.008 PG 15 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 017KO UT WOS:000235692700004 PM 16337183 ER PT J AU Laurance, WF Nascimento, HEM Laurance, SG Andrade, AC Fearnside, PM Ribeiro, JEL Capretz, RL AF Laurance, WF Nascimento, HEM Laurance, SG Andrade, AC Fearnside, PM Ribeiro, JEL Capretz, RL TI Rain forest fragmentation and the proliferation of successional trees SO ECOLOGY LA English DT Article DE Amazon; carbon storage; edge effects; floristic composition; forest dynamics, habitat fragmentation; permanent plots; pioneers; tree communities; tropical forest ID MOIST TROPICAL FOREST; AMAZONIAN FORESTS; NUTRIENT CONCENTRATIONS; HABITAT FRAGMENTATION; POSITIVE FEEDBACKS; SPECIES RICHNESS; BRAZILIAN AMAZON; ATLANTIC FOREST; EDGE; LANDSCAPE AB The effects of habitat fragmentation on diverse tropical tree communities are poorly understood. Over a 20-year period we monitored the density of 52 tree species in nine predominantly Successional genera (Annona, Bellucia, Cecropia, Croton, Goupia, Jacaranada, Miconia, Pourouma, Vismia) in fragmented and continuous Amazonian forests. We also evaluated the relative importance of soil, topographic, forest dynamic, and landscape variables in explaining the abundance and species composition of successional trees. Data were collected within 66 permanent 1-ha plots within a large (similar to 1000 km(2)) experimental landscape, with forest fragments ranging from 1 to 100 ha in area. Prior to forest fragmentation, successional trees were uncommon, typically comprising 2-3% of all trees (>= 10 cm diameter at breast height [1.3 m above the ground surface]) in each plot. Following fragmentation, the density and basal area of successional trees increased rapidly. By 13-17 years after fragmentation, successional trees had tripled in abundance in fragment and edge plots and constituted more than a quarter of all trees in some plots. Fragment age had strong, positive effects on the density and basal area of successional trees, with no indication of a plateau in these variables, suggesting that successional species could become even more abundant in fragments over time. Nonetheless, the 52 species differed greatly in their responses to fragmentation and forest edges. Some disturbance-favoring pioneers (e.g., Cecropia sciadophylla, Vismia guianensis, V. amazonica, V. bemerguii, Miconia cf. crassinervia) increased by > 1000% in density on edge plots, whereas over a third (19 of 52) of all species remained constant or declined in numbers. Species responses to fragmentation were effectively predicted by their median growth rate in nearby intact forest, suggesting that faster-growing species have a strong advantage in forest fragments. An ordination analysis revealed three main gradients in successional-species composition across our study area. Species gradients were most strongly influenced by the stand-level rate of tree mortality on each plot and by the number of nearby forest edges. Species composition also varied significantly among different cattle ranches, which differed in their Surrounding matrices and disturbance histories. These same variables were also the best predictors of total successional-tree abundance and species richness. Successional-tree assemblages in fragment interior plots (> 150 m from edge), which are subjected to fragment area effects but not edge effects, did not differ significantly from those in intact forest, indicating that area effects per se had little influence on Successional trees. Soils and topography also had little discernable effect on these species. Collectively, our results indicate that successional-tree species proliferate rapidly in fragmented Amazonian forests, largely as a result of chronically elevated tree mortality near forest edges and possibly an increased seed rain from successional plants growing in nearby degraded habitats. The proliferation of fast-growing successional trees and correlated decline of old-growth trees will have important effects on species composition, forest dynamics, carbon storage, and nutrient cycling in fragmented forests. C1 Smithsonian Trop Res Inst, Balboa, Panama. INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. INPA, Dept Econ, BR-69011970 Manaus, AM, Brazil. INPA, Dept Bot, BR-69011970 Manaus, AM, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. EM laurancew@si.edu RI Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Fearnside, Philip/D-6559-2011; Laurance, Susan/G-6021-2011; Lahoz da Silva Ribeiro, Jose Eduardo/A-8574-2013 OI Fearnside, Philip/0000-0003-3672-9082; Laurance, Susan/0000-0002-2831-2933; Lahoz da Silva Ribeiro, Jose Eduardo/0000-0002-2389-5631 NR 91 TC 163 Z9 171 U1 13 U2 82 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 FEB PY 2006 VL 87 IS 2 BP 469 EP 482 DI 10.1890/05-0064 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 024SC UT WOS:000236215400022 PM 16637371 ER PT J AU Sack, L Frole, K AF Sack, L Frole, K TI Leaf structural diversity is related to hydraulic capacity in tropical rain forest trees SO ECOLOGY LA English DT Article DE Barro Colorado Island Nature Monument (BCI); biological networks; high pressure flow meter (HPFM); leaf hydraulics; Panama; rain forest trees; shade tolerance; vasculature ID STOMATAL CONDUCTANCE; SHADE TOLERANCE; XYLEM CONDUITS; WOODY-PLANTS; WATER-FLOW; ARCHITECTURE; RESISTANCE; TRAITS; LEAVES; VENATION AB The hydraulic resistance of the leaf (R(1)) is a major bottleneck ill the whole plant water transport pathway and may thus be linked with the enormous Variation ill leaf structure and function among tropical rain forest trees. A previous study found that R(1) varied by an order of magnitude across 10 tree species of Panamanian tropical lowland rain forest. Here, correlations were tested between R(1) and 24 traits relating to leaf venation and mesophyll structure, and to gross leaf form. Across species, R(1) was related to both venation architecture and mesophyll structure. R(1) was positively related to the theoretical axial resistivity of the midrib, determined from xylem conduit numbers and dimensions, and R, was negatively related to venation density in nine of 10 species. R(1) was also negatively related to both palisade mesophyll thickness and to the ratio of palisade to spongy mesophyll. By contrast, numerous leaf traits were independent of R(1) including area, shape, thickness, and density, demonstrating that leaves call be diverse in gross structure without intrinsic trade-offs in hydraulic capacity. Variation in both R(1)-linked and R(1)-independent traits related strongly to regeneration irradiance, indicating the potential importance of both types of traits in establishment ecology. C1 Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Sack, L (reprint author), Univ Hawaii Manoa, Dept Bot, 3190 Maile Way, Honolulu, HI 96822 USA. EM Lsack@hawaii.edu RI Sack, Lawren/A-5492-2008 OI Sack, Lawren/0000-0002-7009-7202 NR 43 TC 163 Z9 182 U1 9 U2 63 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 FEB PY 2006 VL 87 IS 2 BP 483 EP 491 DI 10.1890/05-0710 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 024SC UT WOS:000236215400023 PM 16637372 ER PT J AU Turner, BL Newman, S Newman, JM AF Turner, BL Newman, S Newman, JM TI Organic phosphorus sequestration in subtropical treatment wetlands SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID SOIL-PHOSPHORUS; NORTHERN EVERGLADES; EUTROPHICATION GRADIENT; INOSITOL HEXAPHOSPHATE; NUTRIENT ACCUMULATION; PHOSPHATES; EXTRACTION; SEDIMENTS; FORMS; WATER AB Diffuse phosphorus pollution is commonly remediated by diverting runoff through treatment wetlands to sequester phosphorus into soil layers. Much of the sequestered phosphorus occurs in organic forms, yet our understanding of its chemical nature is limited. We used NaOH-EDTA extraction and solution P-31 NMR spectroscopy to speciate organic phosphorus sequestered in a large treatment wetland (STA-1W) in Florida, USA. The wetland was constructed on previously farmed peat and was designed to remove phosphorus from agricultural runoff prior to discharge into the Everglades. Unconsolidated benthic floc that had accumulated during the 9-year operation of the wetland was sampled along transacts through two connected cells dominated by cattail (Typha dominigensis Pars.) and an additional cell colonized by submerged aquatic vegetation, including southern water nymph (Najas guadalupensis(Spreng.) Magnus) and coontail (Ceratophyllum demersum L.). Organic phosphorus was a greater proportion of the sequestered phosphorus in the cattail marsh compared to the submerged aquatic vegetation wetland, but occurred almost exclusively as phosphate diesters and their alkaline hydrolysis products. It was therefore markedly different from the organic phosphorus in mineral soils, which is dominated typically by inositol phosphates. Phosphate diesters are readily degradable in most soils, raising concern about the long-term fate of organic phosphorus in treatment wetlands. Further studies are now necessary to assess the stability of the sequestered organic phosphorus in response to biogeochemical and hydrological perturbation. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. S FLorida Water Management, Everglades Div, W Palm Beach, FL 33406 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 48 TC 37 Z9 38 U1 3 U2 27 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 FEB 1 PY 2006 VL 40 IS 3 BP 727 EP 733 DI 10.1021/es0516256 PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 010WC UT WOS:000235227600023 PM 16509310 ER PT J AU George, TS Turner, BL Gregory, PJ Cade-Menun, BJ Richardson, AE AF George, TS Turner, BL Gregory, PJ Cade-Menun, BJ Richardson, AE TI Depletion of organic phosphorus from Oxisols in relation to phosphatase activities in the rhizosphere SO EUROPEAN JOURNAL OF SOIL SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Rhizosphere -Perspectives and Challenges CY SEP, 2004 CL Munich, GERMANY ID PLANT-AVAILABLE PHOSPHORUS; SOIL MICROBIAL BIOMASS; P-31 NMR-SPECTROSCOPY; EXTRACELLULAR PHYTASE; INOSITOL PHOSPHATES; ACID-PHOSPHATASE; EXTRACTS; PASTURE; GROWTH; TRANSFORMATIONS AB Phosphorus (P) deficiency is a major limitation to agricultural production in many parts of the world. It is therefore desirable to identify plants with enhanced abilities to utilize P more efficiently. Exudation of phosphatase from roots may improve P availability, yet there is little direct evidence for this. Here we report the dynamics of organic P in the rhizosphere of plants that have enhanced rhizosphere phosphatase activity. Agroforestry species and transgenic subterranean clover (engineered to produce phytase) were compared with crop and wild-type plant controls, respectively. Depletion of organic P was measured in pools defined by chemical extraction, solution P-31 NMR spectroscopy, and microbial immobilization of radio-isotopic P. Plants that had greater extracellular phosphatase activity depleted more organic P from P-deficient Oxisols than control plants. Depleted organic P forms were primarily phosphate monoesters. Plants with enhanced extracellular phosphatase activity also had access to a pool of soil P that was less isotopically exchangeable. Transgenic subterranean clover that expresses a microbial phytase gene appeared to have greater access to recently immobilized P, whereas plants expressing endogenous phosphatases utilized the unlabelled portion of soil organic P to a greater extent. Collectively, these results indicate that the enhancement of phosphatase activity in the rhizosphere of plants is implicated in the depletion of organic P forms from soils, most notably orthophosphate monoesters, whilst also suggesting that there is some exclusivity to the pools of organic P utilized by plants and microorganisms. C1 CSIRO Plant Ind, Canberra, ACT 2601, Australia. Smithsonian Trop Res Inst, Balboa, Alcon, Panama. Scottish Crop Res Inst, Dundee DD2 5DA, Scotland. Stanford Univ, Dept Geog & Environm Sci, Stanford, CA 94305 USA. RP George, TS (reprint author), CSIRO Plant Ind, GPO Box 1600, Canberra, ACT 2601, Australia. EM tim.george@csiro.au RI Turner, Benjamin/E-5940-2011; Richardson, Alan/I-1903-2012; OI Turner, Benjamin/0000-0002-6585-0722; Cade-Menun, Barbara/0000-0003-4391-3718 NR 49 TC 57 Z9 62 U1 7 U2 39 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1351-0754 J9 EUR J SOIL SCI JI Eur. J. Soil Sci. PD FEB PY 2006 VL 57 IS 1 BP 47 EP 57 DI 10.1111/j.1365-2389.2005.00767.x PG 11 WC Soil Science SC Agriculture GA 006TD UT WOS:000234919300006 ER PT J AU Erickson, DL Fenster, CB AF Erickson, DL Fenster, CB TI Intraspecific hybridization and the recovery of fitness in the native legume Chamaecrista fasciculata SO EVOLUTION LA English DT Article DE Chamaecrista fasciculata; epistasis; fitness; heterosis; hybridization; inbreeding depression; recombination ID PITCHER-PLANT MOSQUITO; GENETIC-STRUCTURE; WYEOMYIA-SMITHII; DROSOPHILA-PSEUDOOBSCURA; OUTBREEDING DEPRESSION; NATURAL-POPULATIONS; HYBRID SPECIATION; WILD SUNFLOWERS; EPISTASIS; EVOLUTION AB Genetic incompatibilities and low offspring fitness are characteristic outcomes of hybridization between species. Yet, the creative potential of recombination following hybridization continues to be debated. Here we quantify the outcome of hybridization and recombination between adaptively divergent populations of the North American legume Chamaecrista fasciculata in a large-scale field experiment. Previously, hybrids between these populations demonstrated hybrid breakdown, suggesting the expression of adaptive epistatic interactions underlying population genetic differentiation. However, the outcome of hybridization ultimately rests on the performance of even later generation recombinants. In experiments that compared the performance of recombinant F-6 and F-2 generations with nonrecombinant F-1 and parental genotypes, we observed that increasing recombination had contrasting effects on different life-history components. Lifetime fitness, defined as the product of survivorship and reproduction, showed a strong recovery of fitness in the F-6. The overall gain in fitness with increased recombination suggests that hybridization and recombination may provide the necessary genetic variation for adaptive evolution within species. We discuss the mechanisms that may account for the gain in fitness with recombination, and explore the implications for hybrid speciation and phenotypic evolution. C1 Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Erickson, DL (reprint author), Smithsonian Inst, Lab Analyt Biol, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM derickso@lab.si.edu; cfenster@umd.edu NR 55 TC 60 Z9 62 U1 0 U2 14 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD FEB PY 2006 VL 60 IS 2 BP 225 EP 233 PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 026ZW UT WOS:000236383200002 PM 16610315 ER PT J AU Sundqvist, AK Bjornerfeldt, S Leonard, JA Hailer, F Hedhammar, A Ellegren, H Vila, C AF Sundqvist, AK Bjornerfeldt, S Leonard, JA Hailer, F Hedhammar, A Ellegren, H Vila, C TI Unequal contribution of sexes in the origin of dog breeds SO GENETICS LA English DT Article ID MULTILOCUS GENOTYPE DATA; MITOCHONDRIAL-DNA; DOMESTIC DOG; MICROSATELLITE MARKERS; MORPHOLOGICAL CHANGE; HORSE DOMESTICATION; WILD CANIDS; POPULATION; INFERENCE; IDENTIFICATION AB Dogs (Canis familiaris) were domesticated from the gray wolf (Cams lupus) at least 14,000 years ago, and there is evidence of dogs with phenotypes similar to those in modern breeds 4000 years ago. However, recent genetic analyses have suggested that modern clog breeds have a much snore recent origin, probably <200 years ago. To study the origin of contemporaneous breeds we combined the analysis of paternally inherited Y chromosome markers with maternally inherited mitochondrial DNA and biparentally inherited autosomal microsatellite markers in both domestic dogs and their wild ancestor; the gray wolf. Our results show a sex bias in the origin of breeds, with fewer males than females contributing genetically, which clearly differs froth the breeding patterns in wild gray wolf populations where both sexes have similar contributions. Furthermore, a comparison of mitochondrial DNA and Y chromosome diversity in dog groups recognized by the World Canine Organization, as well as in groups defined by the breeds' genetic composition, shows that paternal lineages are more differentiated among groups than maternal lineages. This demonstrates a lower exchange of males than of females between breeds belonging to different groups, which illustrates how breed founders may have been chosen. C1 Uppsala Univ, Dept Evolutionary Biol, SE-75236 Uppsala, Sweden. Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Genet Program, Washington, DC 20008 USA. Swedish Univ Agr Sci, Dept Small Anim Clin Sci, SE-75007 Uppsala, Sweden. RP Sundqvist, AK (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18 D, SE-75236 Uppsala, Sweden. EM anna-karin.sundqvist@ebc.uu.se RI Hailer, Frank/C-9114-2012; Vila, Carles/H-4893-2013; Leonard, Jennifer/A-7894-2010 OI Hailer, Frank/0000-0002-2340-1726; Vila, Carles/0000-0002-4206-5246; Leonard, Jennifer/0000-0003-0291-7819 NR 50 TC 53 Z9 57 U1 1 U2 30 PU GENETICS PI BALTIMORE PA 428 EAST PRESTON ST, BALTIMORE, MD 21202 USA SN 0016-6731 J9 GENETICS JI Genetics PD FEB PY 2006 VL 172 IS 2 BP 1121 EP 1128 DI 10.1534/genetics.105.042358 PG 8 WC Genetics & Heredity SC Genetics & Heredity GA 024ER UT WOS:000236178800035 PM 16219789 ER PT J AU Watters, TR McGovern, PJ AF Watters, TR McGovern, PJ TI Lithospheric flexure and the evolution of the dichotomy boundary on Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CRUSTAL DICHOTOMY; PLATE-TECTONICS; LOBATE SCARPS; THRUST FAULTS; GRAVITY; TOPOGRAPHY; LOWLANDS; ORIGIN; MANTLE AB The boundary of the Martian crustal dichotomy in the eastern hemisphere is one of the most striking topographic features on the planet. The long wavelength topography of much of the boundary is expressed by a broad rise and an arched ramp that slopes downward from the southern highlands into the northern lowlands and often ends in a steep scarp. Lithospheric flexure of the southern highlands for both a continuous and broken plate boundary with the northern lowlands lithosphere is modeled. We find that the long wavelength topography of the boundary is best fit by a lithospheric deflection profile of a broken lithosphere for reasonable values of the flexural parameter. The lithosphere near the dichotomy boundary may have been weakened by tectonic stress associated with the formation of the crustal dichotomy by subcrustal transport caused by overturn of an early magma ocean. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watters@si.edu NR 33 TC 14 Z9 14 U1 0 U2 0 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 FEB 1 PY 2006 VL 33 IS 8 AR L08S05 DI 10.1029/2005GL024325 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 010BA UT WOS:000235157000001 ER PT J AU Altshuler, DL Dudley, R AF Altshuler, DL Dudley, R TI Adaptations to life at high elevation: An introduction to the symposium SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Editorial Material C1 CALTECH, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Altshuler, DL (reprint author), CALTECH, Mail Code 138-78,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM doug@caltech.edu NR 12 TC 2 Z9 2 U1 1 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2006 VL 46 IS 1 BP 3 EP 4 DI 10.1093/icb/icj002 PG 2 WC Zoology SC Zoology GA 012KC UT WOS:000235337100002 PM 21672717 ER PT J AU Dillon, ME Frazier, MR Dudley, R AF Dillon, ME Frazier, MR Dudley, R TI Into thin air: Physiology and evolution of alpine insects SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol ID ORCHID BEES APIDAE; BODY-SIZE; SPECIES RICHNESS; ELEVATIONAL GRADIENTS; DROSOPHILA-MELANOGASTER; OXYGEN LIMITATION; LIFE-HISTORY; ALTITUDINAL GRADIENT; REARING TEMPERATURE; NATURAL-POPULATIONS AB Synopsis Numerous physical parameters that influence insect physiology vary Substantially with altitude, including temperature, air density, and oxygen partial pressure. Here, we review existing literature and present new empirical data to better characterize the high-altitude environment, and then consider how this environment affects the physiology and evolution of insects. Using weather balloon data from fifty-three sites across the globe, we estimate a mean altitudinal temperature lapse rate of 6.0 degrees C/km. We also present empirically determined lapse rates for P, and air density. The temperature decline with elevation may substantially compromtise insect thermoregulation at high altitude. However, heat-transfer models predict that lower air density at elevation reduces convective heat loss of insects by to a surprisingly large degree. This effect combined with behavioral thermo regulation and the availability of buffered microhabitats make the net thermal consequences of highaltitude residence strongly context-specific. The decline in Po, with elevation may compromise insect development and physiology, but its effects are difficult to predict without simultaneously considering temperature and air density. Flying insects compensate for low air densities with both short-term responses, Such as increased stroke amplitude (but not wingbeat frequency), and with long-term developmental and/or evolutionary increases in wing size relative to body size. Finally, in contrast to predictions based on Bergmann's Rule, a literature survey of thirty-six insect species suggests that those living in colder, higher altitudes do not tend to have larger body sizes. C1 Univ Washington, Dept Biol, Seattle, WA 98195 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Dillon, ME (reprint author), Univ Washington, Dept Biol, Box 351800, Seattle, WA 98195 USA. EM dillonm@u.washington.edu RI Frazier, Melanie/A-2367-2012; Dillon, Michael/A-2564-2012 OI Dillon, Michael/0000-0002-7263-5537 NR 100 TC 82 Z9 83 U1 3 U2 46 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2006 VL 46 IS 1 BP 49 EP 61 DI 10.1093/icb/icj007 PG 13 WC Zoology SC Zoology GA 012KC UT WOS:000235337100007 PM 21672722 ER PT J AU Altshuler, DL Dudley, R AF Altshuler, DL Dudley, R TI The physiology and biomechanics of avian flight at high altitude SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol ID PARABRONCHIAL GAS-EXCHANGE; HOVERING INSECT FLIGHT; BAR-HEADED GEESE; HUMMINGBIRD FLIGHT; MIGRATING BIRDS; OXYGEN-CONSUMPTION; WATER-BALANCE; WIND; PERFORMANCE; ENERGETICS AB Synopsis Many birds fly at high altitude, either during long-distance flights or by virtue of residence in high-elevation habitats. Among the many environmental features that vary systematically with altitude, five have significant consequences for avian flight performance: ambient wind speeds, air temperature, humidity, oxygen availability, and air density. During migratory flights, birds select flight altitudes that minimize energy expenditure via selection of advantageous tail- and crosswinds. Oxygen partial pressure decreases substantially to as little as 26% of sea-level values for the highest altitudes at which birds migrate, whereas many taxa reside above 3000 meters in hypoxic air. Birds exhibit numerous adaptations in pulmonary, cardiovascular, and muscular systems to alleviate such hypoxia. The systematic decrease in air density with altitude can lead to a benefit for forward flight through reduced drag but imposes an increased aerodynamic demand for hovering by degrading lift production and simultaneously elevating the induced power requirements of flight. This effect has been well-studied in the hovering flight of hummingbirds, which Occur throughout high-elevation habitats in the western hemisphere. Phylogenetically controlled studies have shown that hummingbirds compensate morphologically for Such hypodense air through relative increases in wing size, and kinematically via increased stroke amplitude during the wingbeat. Such compensatory mechanisms result in fairly constant power requirements for hovering at different elevations, but decrease the margin of excess power available for other flight behaviors. C1 CALTECH, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Altshuler, DL (reprint author), CALTECH, Mail Code 138-78,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM doug@caltech.edu NR 86 TC 34 Z9 35 U1 9 U2 59 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD FEB PY 2006 VL 46 IS 1 BP 62 EP 71 DI 10.1093/icb/icj008 PG 10 WC Zoology SC Zoology GA 012KC UT WOS:000235337100008 PM 21672723 ER PT J AU Gingerich, O AF Gingerich, O TI The Toledan Tables. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 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 FEB PY 2006 VL 37 BP 116 EP 117 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 013YB UT WOS:000235444800011 ER PT J AU Riede, T Bronson, E Hatzikirou, H Zuberbuhler, K AF Riede, T Bronson, E Hatzikirou, H Zuberbuhler, K TI Multiple discontinuities in nonhuman vocal tracts - A response to Lieberman (2006) SO JOURNAL OF HUMAN EVOLUTION LA English DT Editorial Material ID TONGUE MOVEMENT; LARYNGEAL POSITION; CT-SCANS; CAT; VOCALIZATION; EVOLUTION; APPARATUS; PHARYNX; SPEECH; LENGTH C1 Univ Wisconsin, Dept Surg, Madison, WI 53706 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Tech Univ Dresden, Ctr Informat Serv & High Performance Comp, D-01062 Dresden, Germany. Univ St Andrews, Sch Psychol, St Andrews KY16 9AJ, Fife, Scotland. RP Riede, T (reprint author), Univ Wisconsin, Dept Surg, 5745 Med Sci, Madison, WI 53706 USA. EM tobiasriede@web.de RI Zuberbuhler, Klaus/A-9053-2011; Riede, Tobias/J-9092-2012; OI Zuberbuhler, Klaus/0000-0001-8378-088X; Riede, Tobias/0000-0001-6875-0017; Riede, Tobias/0000-0001-9606-0742 NR 45 TC 11 Z9 12 U1 0 U2 3 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD FEB PY 2006 VL 50 IS 2 BP 222 EP 225 DI 10.1016/j.jhevol.2005.10.005 PG 4 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 017CC UT WOS:000235670700008 ER PT J AU Grady, FV Olson, SL AF Grady, FV Olson, SL TI Fossil bats from quaternary deposits on Bermuda (Chiroptera : Vespertilionidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE bat; Bermuda; Chiroptera; fossil; Holocene; Lasiurus; paleontology; Pipistrellus; Pleistocene; quaternary ID STRATIGRAPHY AB Fossil remains of bats have been recovered from caves and fissures in Bermuda dating from middle Pleistocene to late Holocene. Three bones from 2 different localities are identified as eastern pipistrelle (Pipistrellus subflavus), which was not recorded from Bermuda until 2004. Remains of an individual eastern red bat (Lasiurus borealis), from a 400,000-year-old beach deposit, imply that the migratory pattern in this species, a regular transient in Bermuda today, may have been established by the middle Pleistocene. Fairly common remains of Lasiurus, either L. borealis or L. senfinolus, were found in 5 cave deposits. In I finely stratified sequence, this bat does not appear until the onset of the last glacial period, suggesting that a resident population may have become established at that time. A strong taphonomic bias, indicated by the preponderance of large wing bones, probably of females, may be the result of hawk predation. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM olsons@si.edu NR 16 TC 12 Z9 12 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 FEB PY 2006 VL 87 IS 1 BP 148 EP 152 DI 10.1644/05-MAMM-A-179R1.1 PG 5 WC Zoology SC Zoology GA 019OB UT WOS:000235845500022 ER PT J AU Savov, IP Hickey-Vargas, R D'Antonio, M Ryan, JG Spadea, P AF Savov, IP Hickey-Vargas, R D'Antonio, M Ryan, JG Spadea, P TI Petrology and geochemistry of West Philippine Basin basalts and early Palau-Kyushu arc volcanic clasts from ODP Leg 195, site 1201D: Implications for the early history of the Izu-Bonin-Mariana arc SO JOURNAL OF PETROLOGY LA English DT Article DE back-arc basalts; Izu-Bonin-Marianas; Philippine Sea; subduction initiation; Ocean Drilling Program Leg 195 ID SEA PLATE; ISOTOPE EVIDENCE; RIDGE BASALTS; FORE-ARC; ORIGIN; EVOLUTION; ELEMENT; CONSTRAINTS; MAGMAS; EOCENE AB Site 1201D of Ocean Drilling Program Leg 195 recovered basaltic and volcaniclastic units from the West Philippine Basin that document the earliest history of the Izu-Bonin-Mariana convergent margin. The stratigraphic section recovered at Site 1201D includes 90 m of pillow basalts, representing the West Philippine Basin basement, overlain by 459 m of volcaniclastic turbidites that formed from detritus shed from the Eocene-Oligocene proto-Izu-Bonin-Mariana island arc. Basement basalts are normal mid-ocean ridge basalt (N-MORB), based on their abundances of immobile trace elements, although fluid-mobile elements are enriched, similar to back-arc basin basalts (BABB). Sr, Nd, Pb and Hf isotopic compositions of the basement basalts are similar to those of basalts from other West Philippine Basin locations, and show an overall Indian Ocean MORB signature, marked by high Pb-208/Pb-204 for a given Pb-206/Pb-204 and high Hf-176/Hf-177 for a given Nd-143/Nd-144. Trace element and isotopic differences between the basement and overlying arc-derived volcaniclastics are best explained by the addition of subducted sediment or sediment melt, together with hydrous fluids from subducted oceanic crust, into the mantle source of the arc lavas. In contrast to tectonic models suggesting that a mantle hotspot was a source of heat for the early Izu-Bonin-Mariana arc magmatism, the geochemical data do not support an enriched, ocean island basalt (OIB)-like source for either the basement basalts or the arc volcanic section. C1 Univ S Florida, Dept Geol, Tampa, FL 33620 USA. Florida Int Univ, Dept Earth Sci, Miami, FL 33199 USA. Univ Naples Federico II, Dipartimento Sci Terra, I-80138 Naples, Italy. Ist Nazl Geofis & Vulcanol, Osservatorio Vesuviano, Naples, Italy. Univ Udine, Dipartimento Georisorse & Terr, I-33100 Udine, Italy. RP Savov, IP (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,NHB-119, Washington, DC 20013 USA. EM savovi@si.edu RI D'Antonio, Massimo/C-5199-2012 OI D'Antonio, Massimo/0000-0003-2077-943X NR 50 TC 30 Z9 31 U1 1 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 EI 1460-2415 J9 J PETROL JI J. Petrol. PD FEB PY 2006 VL 47 IS 2 BP 277 EP 299 DI 10.1093/petrology/egi075 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 004WN UT WOS:000234783400003 ER PT J AU Sharrer, T AF Sharrer, T TI Tapping the pines: The naval stores industry in the American South. SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sharrer, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOUTHERN HISTORICAL ASSOC PI ATHENS PA UNIV GEORGIA, HISTORY DEPT, ATHENS, GA 30602 USA SN 0022-4642 J9 J SOUTHERN HIST JI J. South. Hist. PD FEB PY 2006 VL 72 IS 1 BP 169 EP 170 PG 2 WC History SC History GA 011SA UT WOS:000235287200023 ER PT J AU Chust, G Chave, J Condit, R Aguilar, S Lao, S Perez, R AF Chust, G Chave, J Condit, R Aguilar, S Lao, S Perez, R TI Determinants and spatial modeling of tree beta-diversity in a tropical forest landscape in Panama SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE dispersal limitation; neutral hypothesis; Panama; remote sensing; species similarity; variation partitioning ID FLORISTIC PATTERNS; COLOMBIAN AMAZONIA; SPECIES-DIVERSITY; RAIN-FOREST; BIODIVERSITY; DOMINANCE; GRADIENT; HOTSPOTS; DESIGN; BORNEO AB Questions: The objectives of this study were to clarify the extent to which environmental factors and geographical distance account for tropical floristic composition, and propose a methodology for delimiting the boundaries of floristic types based on species similarity. Location: The Panama Canal watershed. Methods: To assess which factors (climate, topography, geology and geographical distance) account for floristic composition, we performed Mantel tests on distance matrices and partitioned variation in species composition using canonical analysis. We used a permutation-based regression model computed on distance matrices and a hierarchical clustering of the tree composition to construct a predictive map of forest types of the Panama Canal Watershed. Results: We found that spatial variation alone explained 22-27% of species variation, while the fraction of species variation explained by environmental variables was smaller (10-12%); 13-19% of the variation was accounted for by the joint effect of environmental variation and geographic distance. The similarity-based map emphasizes the principal division in tree flora between the drier Pacific side and the wetter Caribbean slopes. Conclusions: The distribution of Panamanian tree species appears to be primarily determined by dispersal limitation, then by environmental heterogeneity. 'Environmental segregation' processes do play an important role. Maps of broad-scale vegetation patterns based on thorough tree inventories can be used in conservation planning in the tropics. C1 Univ Toulouse 3, CNRS, Lab Evolut & Divers Biol, F-31062 Toulouse, France. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Miami, FL 34002 USA. RP Chave, J (reprint author), Univ Toulouse 3, CNRS, Lab Evolut & Divers Biol, Batiment 4R3,118 Route Narbonne, F-31062 Toulouse, France. EM chave@cict.fr RI Chust, Guillem/C-1112-2008 OI Chust, Guillem/0000-0003-3471-9729 NR 49 TC 57 Z9 60 U1 4 U2 45 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 FEB PY 2006 VL 17 IS 1 BP 83 EP 92 DI 10.1111/j.1654-1103.2006.tb02426.x PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 017BN UT WOS:000235669200011 ER PT J AU Riley, S AF Riley, S TI Dog days. 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 FEB 1 PY 2006 VL 131 IS 2 BP 69 EP 69 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 006XH UT WOS:000234930500054 ER PT J AU Schroll, CS AF Schroll, CS TI Francis Bacon's studio. SO LIBRARY JOURNAL LA English DT Book Review C1 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 FEB 1 PY 2006 VL 131 IS 2 BP 75 EP 75 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 006XH UT WOS:000234930500090 ER PT J AU Smith, DA Ralls, K Hurt, A Adams, B Parker, M Maldonado, JE AF Smith, DA Ralls, K Hurt, A Adams, B Parker, M Maldonado, JE TI Assessing reliability of microsatellite genotypes from kit fox faecal samples using genetic and GIS analyses SO MOLECULAR ECOLOGY LA English DT Article DE endangered species; faecal analysis; faecal genotypes; kit fox; noninvasive sampling; scats; Vulpes macrotis mutica ID VULPES-MACROTIS-MUTICA; ESTIMATING POPULATION-SIZE; NATURAL-POPULATIONS; MOLECULAR TRACKING; NONINVASIVE METHOD; ELUSIVE ANIMALS; CANIS-LATRANS; MELES-MELES; LATRINE USE; FECES AB Noninvasive faecal DNA sampling has the potential to provide a wealth of information necessary for monitoring and managing endangered species while eliminating the need to capture, handle or observe rare individuals. However, scoring problems, and subsequent genotyping errors, associated with this monitoring method remain a great concern as they can lead to misidentification of individuals and biased estimates. We examined a kit fox scat data set (353 scats; 80 genotypes) for genotyping errors using both genetic and GIS analyses, and evaluated the feasibility of combining both approaches to assess reliability of the faecal DNA results. We further checked the appropriateness of using faecal genotypes to study kit fox populations by describing information about foxes that we could deduce from the 'acceptable' scat genotypes, and comparing it to information gathered with traditional field techniques. Overall, genetic tests indicated that our data set had a low rate of genotyping error. Furthermore, examination of distributions of scat locations confirmed our data set was relatively error free. We found that analysing information on sex primer consistency and scat locations provided a useful assessment of scat genotype error, and greatly limited the amount of additional laboratory work that was needed to identify potentially 'false' scores. 'Acceptable' scat genotypes revealed information on sex ratio, relatedness, fox movement patterns, latrine use, and size of home range. Results from genetic and field data were consistent, supporting the conclusion that our data set had a very low rate of genotyping error and that this noninvasive method is a reliable approach for monitoring kit foxes. C1 Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. Smithsonian Inst, Natl Zool Pk, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Univ Montana, Sch Forestry, Wildlife Biol Program, Missoula, MT 59812 USA. RP Smith, DA (reprint author), Univ Washington, Dept Ecosyst Sci, Seattle, WA 98195 USA. EM debsmith@u.washington.edu NR 54 TC 36 Z9 39 U1 1 U2 18 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 2006 VL 15 IS 2 BP 387 EP 406 DI 10.1111/j.1365-294X.2005.02841.x PG 20 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 008MS UT WOS:000235045500008 PM 16448408 ER PT J AU May-Collado, L Agnarsson, I AF May-Collado, L Agnarsson, I TI Cytochrome b and Bayesian inference of whale phylogeny SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE balaneidae; cetancodonta; cetartiodactyla; delphinidae; delphinoidea; euungulata; iniidae; missing data; mitochondrial DNA; monodentidae; mysticeti; odontoceti; monophyly; perissodactyla; phocenidae; platanistidae; phylogeny; taxon sampling; ziphiidae ID DNA-SEQUENCES; NUCLEOTIDE SUBSTITUTION; MOLECULAR EVIDENCE; CETACEAN LINEAGES; RIVER DOLPHINS; GENE-SEQUENCES; BALEEN WHALES; SPERM-WHALE; MITOCHONDRIAL; ARTIODACTYLS AB In the mid 1990s cytochrome b and other mitochondrial DNA data reinvigorated cetacean phylogenetics by proposing many novel and provocative hypotheses of cetacean relationships. These results sparked a revision and reanalysis of morphological datasets, and the collection of new nuclear DNA data from numerous loci. Some of the most controversial mitochondrial hypotheses have now become benchmark clades, corroborated with nuclear DNA and morphological data; others have been resolved in favor of more traditional views. That major conflicts in cetacean phylogeny are disappearing is encouraging. However, most recent papers aim specifically to resolve higher-level conflicts by adding characters, at the cost of densely sampling taxa to resolve lower-level relationships. No molecular study to date has included more than 33 cetaceans. More detailed molecular phylogenies will provide better tools for evolutionary studies. Until more genes are available for a high number of taxa, can we rely on readily available single gene mitochondrial data? Here, we estimate the phylogeny of 66 cetacean taxa and 24 outgroups based on Cytb sequences. We judge the reliability of our phylogeny based on the recovery of several deep-level benchmark clades. A Bayesian phylogenetic analysis recovered all benchmark clades and for the first time supported Odontoceti monophyly based exclusively on analysis of a single mitochondrial gene. The results recover the monophyly of all but one family level taxa within Cetacea, and most recently proposed super- and subfamilies. In contrast, parsimony never recovered all benchmark clades and was sensitive to a priori weighting decisions. These results provide the most detailed phylogeny of Cetacea to date and highlight the utility of both Bayesian methodology in general, and of Cytb in cetacean phylogenetics. They furthermore suggest that dense taxon sampling, like dense character sampling, can overcome problems in phylogenetic reconstruction. (c) 2005 Elsevier Inc. All rights reserved. C1 Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Washington, DC 20013 USA. RP May-Collado, L (reprint author), Florida Int Univ, Dept Biol Sci, 11200 SW 8th St, Miami, FL 33199 USA. EM lmayc002@fiu.edu; ingi@zoology.ubc.ca NR 98 TC 94 Z9 99 U1 1 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD FEB PY 2006 VL 38 IS 2 BP 344 EP 354 DI 10.1016/j.ympev.2005.09.019 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 009OO UT WOS:000235121800005 PM 16325433 ER PT J AU Roelofs, GHA Groot, PJ Marsh, TR Steeghs, D Nelemans, G Patterson, J AF Roelofs, GHA Groot, PJ Marsh, TR Steeghs, D Nelemans, G Patterson, J TI Phase-resolved spectroscopy of the helium dwarf nova 'SN 2003aw' in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : close; stars : individual : SN 2003aw; stars : individual : SDSS J124058.03; 015919.2; novae, cataclysmic variables ID AM-CVN STAR; BINARIES AB High time resolution spectroscopic observations of the ultracompact helium dwarf nova 'SN 2003aw' in its quiescent state at V similar to 20.5 reveal its orbital period at 2027.8 +/- 0.5 s or 33.80 min. Together with the photometric 'superhump' period of 2041.5 +/- 0.5 s, this implies a mass ratio q approximate to 0.036. We compare both the average and time-resolved spectra of 'SN 2003aw' and Sloan Digital Sky Survey (SDSS) J124058.03-015919.2. Both show a DB white dwarf spectrum plus an optically thin, helium-dominated accretion disc. 'SN 2003aw' distinguishes itself from the SDSS source by its strong calcium H & K emission lines, suggesting higher abundances of heavy metals than the SDSS source. The silicon and iron emission lines observed in the SDSS source are about twice as strong in 'SN 2003aw'. The peculiar 'double bright spot' accretion disc feature seen in the SDSS source is also present in time-resolved spectra of 'SN 2003aw', albeit much weaker. C1 Radboud Univ, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. RP Roelofs, GHA (reprint author), Radboud Univ, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM g.roelofs@astro.ru.nl RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X NR 13 TC 28 Z9 28 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 FEB 1 PY 2006 VL 365 IS 4 BP 1109 EP 1113 DI 10.1111/j.1365-2966.2005.09727.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 006DV UT WOS:000234876600005 ER PT J AU Grindlay, J Zwart, SP McMillan, S AF Grindlay, J Zwart, SP McMillan, S TI Short gamma-ray bursts from binary neutron star mergers in globular clusters SO NATURE PHYSICS LA English DT Article ID 28 FEBRUARY 1997; GLOBULAR-CLUSTER-47 TUCANAE; MILLISECOND PULSAR; RADIO PULSARS; DISCOVERY; EVOLUTION; EMISSION; CHANDRA; GALAXY; M15 AB Observations by the Swift gamma-ray-burst (GRB) mission located short GRBs in (or near) elliptical galaxies, that are no longer active in star formation. This suggested that short GRBs are produced when neutron stars (NSs) merge with other NSs or with black holes (BHs). However, the spatial offset of some short GRBs from their host galaxies is not consistent with double-neutron-star (DNS) systems formed from massive binary stars, which appear to remain in galactic disks. Instead, short GRBs may arise from NS mergers in compact binary systems that are naturally produced in globular clusters, in which extreme densities of very old stars can create and exchange compact binaries efficiently. Here we present a simple scaling from the DNS binary observed in the globular cluster M15 in our own Galaxy to the numbers expected for globular clusters around galaxies generally. We present numerical simulations that demonstrate that DNS production in globular clusters may account for similar to 10-30% of the observed short GRBs. The much more numerous DNS merger rates predicted for galactic disks suggests their associated short GRBs are significantly more beamed, perhaps by the aligned spins and greater magnetic field of their secondary NSs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Sect Computat Sci Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. RP Grindlay, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jgrindlay@cfa.harvard.edu NR 35 TC 94 Z9 94 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD FEB PY 2006 VL 2 IS 2 BP 116 EP 119 DI 10.1038/nphys214 PG 4 WC Physics, Multidisciplinary SC Physics GA 014FM UT WOS:000235464700022 ER PT J AU Seitz, R Raymond, JC Kissel, J Petaev, MI AF Seitz, R Raymond, JC Kissel, J Petaev, MI TI Xenomict energy in cold solids in space SO NATURWISSENSCHAFTEN LA English DT Article ID INTERSTELLAR DUST; ZIRCON; IRRADIATION; MINERALS; COMETS AB Minerals on earth whose crystalline order has been reduced by radioactive decay of contained atoms are termed "metamict." They are rare and few because in most crystalline solids, atoms and vacancies are relatively mobile at terrestrial temperatures, and radiation damage tends to be self-annealing. This is not the case in the extreme cold of deep space. Below roughly 100 K, reduced vacancy mobility allows cosmic ray and solar wind induced lattice defects to endure and accumulate for eons, reaching energy densities of up to MJ k(-1) in some materials. We examine the possible effects of the release of energy stored in cold deep-space materials when solid-state defects recombine upon warming due to impacts, gravitational infall, or perihelion. Dimensional analysis suggests energetic defect recombination in radiation-damaged "xenomict" solids in comets, and planetesimals may, in some circumstances, raise internal temperatures enough to melt ice and volatilize frozen gases. We speculate that this may account for some cometary outbursts and Deep Impact experiment results. Calorimetric experiments on appropriately irradiated natural and synthetic materials are needed to further quantify these mechanisms. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Seitz, R (reprint author), 2 Ware St 507, Cambridge, MA 02138 USA. EM Mnestheus@aol.com NR 19 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2006 VL 93 IS 2 BP 88 EP 91 DI 10.1007/s00114-005-0067-9 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 013XC UT WOS:000235442300006 PM 16362427 ER PT J AU Baker, ME Weller, DE Jordan, TE AF Baker, ME Weller, DE Jordan, TE TI Comparison of automated watershed delineations: Effects on land cover areas, percentages, and relationships to nutrient discharge SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID DIGITAL ELEVATION DATA; MID-ATLANTIC REGION; LANDSCAPE INFLUENCES; STREAM ECOSYSTEMS; CHESAPEAKE BAY; QUALITY; INDICATORS; CATCHMENT; CHEMISTRY; MULTIPLE AB We compared manual delineations with those derived from ten automated delineations of 420 watersheds in four physiographic provinces of the Chesapeake Basin. Automated methods included commercial DEM-based routines and different parameterizations of four enhanced methods: stream burning, normalized excavation, surface reconditioning, and normalized reconditioning. Un-enhanced methods resulted in individual watershed boundaries with some gross discrepancies in watershed size relative to manual delineations (error rate of 0.22 > 25 percent difference compared to manual) and significantly different watershed size distributions (Mann-Whitney U p = 0.012). Integrating mopped streams through enhanced methods substantially improved correspondence with manual watersheds (error rates of only 0.08-0.02 > 25 percent difference). Analysis of cropland area among methods showed a significant difference between manual estimates and un-enhanced estimates (p = 0.049) that was corrected using enhanced algorithms, Subsequent analysis of percent cropland revealed that measurements of land cover proportions were not always affected by delineation errors. However, differences were large enough to influence regressions with stream nitrate-N at the 90 percent confidence level within one physiographic province. Enhanced delineations produced statistical relationships between percent cropland and nitrate-N concentrations consistent with manual delineations. The results provide support for enhanced automated watershed delineation within the Chesapeake Basin and suggest that normalized excavation can be an effective augmentation of existing stream burning and reconditioning procedures. C1 Utah State Univ, Dept Aquat Watershed & Earth Resources, Logan, UT 84322 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Baker, ME (reprint author), Utah State Univ, Dept Aquat Watershed & Earth Resources, 5210 Old Main Hill, Logan, UT 84322 USA. EM matt.baker@usu.edu RI Baker, Matthew/I-2839-2014; OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437 NR 33 TC 28 Z9 30 U1 2 U2 14 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD FEB PY 2006 VL 72 IS 2 BP 159 EP 168 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 014AY UT WOS:000235452300012 ER PT J AU Calzetta, E Hu, BL Rey, AM AF Calzetta, E Hu, BL Rey, AM TI Bose-Einstein-condensate superfluid-Mott-insulator transition in an optical lattice SO PHYSICAL REVIEW A LA English DT Review ID MEAN-FIELD THEORY; TONKS-GIRARDEAU GAS; HUBBARD-MODEL; PHASE-TRANSITION; ULTRACOLD BOSONS; NOBEL LECTURE; ATOMS; DYNAMICS; SYSTEMS; EQUATION AB We present an analytical model for a cold bosonic gas on an optical lattice (with densities of the order of 1 particle per site), targeting the critical regime of the Bose-Einstein-condensate superfluid-Mott-insulator transition. We focus on the computation of the one-body density matrix and its Fourier transform, the momentum distribution which is directly obtainable from "time-of-flight" measurements. The expected number of particles with zero momentum may be identified with the condensate population if it is close to the total number of particles. Our main result is an analytic expression for this observable, interpolating between the known results valid for the two regimes separately: the standard Bogoliubov approximation valid in the superfluid regime and the strong-coupling perturbation theory valid in the Mott regime. C1 Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Fis, RA-1428 Buenos Aires, DF, Argentina. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Fis, Ciudad Univ, RA-1428 Buenos Aires, DF, Argentina. NR 132 TC 9 Z9 9 U1 3 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2006 VL 73 IS 2 AR 023610 DI 10.1103/PhysRevA.73.023610 PG 18 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 017BC UT WOS:000235668100157 ER PT J AU Rey, AM Pupillo, G Porto, JV AF Rey, AM Pupillo, G Porto, JV TI The role of interactions, tunneling, and harmonic confinement on the adiabatic loading of bosons in an optical lattice SO PHYSICAL REVIEW A LA English DT Article ID TONKS-GIRARDEAU GAS; ATOMS; SYSTEMS AB We calculate entropy-temperature curves for interacting bosons in unit filled optical lattices for both homogeneous and harmonically trapped situations, and use them to understand how adiabatic changes in the lattice depth affect the temperature of the system. In a translationally invariant lattice, the zero tunneling limit facilitates a rather detailed analytic description. Unlike the noninteracting bosonic system which is always cooled upon adiabatic loading for low enough initial temperature, the change in the excitation spectrum induced by interactions can lead to heating. Finite tunneling helps to reduce this heating. Finally, we study the spatially inhomogeneous system confined in a parabolic potential and show that the presence of the trap can significantly reduce the final available temperature, due to the nonvanishing superfluid component at the edge of the cloud which is present in trapped systems. C1 Natl Inst Standards & Technol, Gaithersburg, MD 20899 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Natl Inst Standards & Technol, Gaithersburg, MD 20899 USA. EM arey@cfa.harvard.edu NR 25 TC 26 Z9 26 U1 1 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2006 VL 73 IS 2 AR 023608 DI 10.1103/PhysRevA.73.023608 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 017BC UT WOS:000235668100155 ER PT J AU Zhang, JY Yan, ZC Vrinceanu, D Babb, JF Sadeghpour, HR AF Zhang, JY Yan, ZC Vrinceanu, D Babb, JF Sadeghpour, HR TI Long-range interactions between a He(2 S-3) atom and a He(2 P-3) atom for like isotopes SO PHYSICAL REVIEW A LA English DT Article ID ULTRACOLD METASTABLE HELIUM; SCATTERING LENGTH AB For the interactions between a He(2 S-3) atom and a He(2 P-3) atom for like isotopes, we report perturbation theoretic calculations using accurate variational wave functions in Hylleraas coordinates of the coefficients determining the potential energies at large internuclear separations. We evaluate the coefficient C-3 of the first order resonant dipole-dipole energy and the van der Waals coefficients C-6, C-8, and C-10 for the second order energies arising from the mutual perturbations of instantaneous electric dipole, quadrupole, and octupole interactions. We also evaluate the leading contribution to the third-order energy. We establish definitive values including treatment of the finite nuclear mass for the He-3(2 S-3)-He-3(2 P-3) and He-4(2 S-3)-He-4(2 P-3) interactions. C1 Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. Los Alamos Natl Lab, T4 Grp, Los Alamos, NM 87545 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. RI Yan, Zong-Chao/F-6668-2014 NR 15 TC 16 Z9 16 U1 1 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2006 VL 73 IS 2 AR 022710 DI 10.1103/PhysRevA.73.022710 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 017BC UT WOS:000235668100107 ER PT J AU Saunders, CJ Megonigal, JP Reynolds, JF AF Saunders, CJ Megonigal, JP Reynolds, JF TI Comparison of belowground biomass in C-3- and C-4-dominated mixed communities in a Chesapeake Bay brackish marsh SO PLANT AND SOIL LA English DT Article DE brackish marsh; C-3; C-4; Chesapeake Bay; rhizome; root; stable carbon isotope ID ELEVATED ATMOSPHERIC CO2; GRASS SPARTINA-PATENS; DUNE SLACK PLANT; SALT-MARSH; PHRAGMITES-AUSTRALIS; METABOLIC RESPONSES; SCIRPUS-AMERICANUS; CLIMATE-CHANGE; ROOT TURNOVER; GAS-EXCHANGE AB Below ground biomass is a critical factor regulating ecosystem functions of coastal marshes, including soil organic matter (SOM) accumulation and the ability of these systems to keep pace with sea-level rise. Nevertheless, below ground biomass responses to environmental and vegetation changes have been given little emphasis marsh studies. Here we present a method using stable carbon isotopes and color to identify root and rhizomes of Schoenoplectus americanus (Pers.) Volk. ex Schinz and R. Keller (C-3) and Spartina patens (Ait.) Muhl. (C-4) occurring in C-3- and C-4-dominated communities in a Chesapeake Bay brackish marsh. The functional significance of the biomass classes we identified is underscored by differences in their chemistry, depth profiles, and variation in biomass and profiles relative to abiotic and biotic factors. C-3 rhizomes had the lowest concentrations of cellulose (29.19%) and lignin (14.43%) and the lowest C:N (46.97) and lignin:N (0.16) ratios. We distinguished two types of C-3 roots, and of these, the dark red C-3 roots had anomalously high C:N (195.35) and lignin:N (1.14) ratios, compared with other root and rhizome classes examined here and with previously published values. The C-4-dominated community had significantly greater below ground biomass (4119.1 g m(-2)) than the C-3-dominated community (3256.9 g m(-2)), due to greater total root biomass and a 3.6-fold higher C-3-root:rhizome ratio in the C-4-dominated community. C-3 rhizomes were distributed significantly shallower in the C-4-dominated community, while C-3 roots were significantly deeper. Variability in C3 rhizome depth distributions was explained primarily by C-4 biomass, and C-3 roots were explained primarily by water table height. Our results suggest that below ground biomass in this system is sensitive to slight variations in water table height (across an 8 cm range), and that the reduced overlap between C-3 and C-4 root profiles in the C-4-dominated community may account for the greater total root biomass observed in that community. Given that future elevated atmospheric CO2 and accelerated sea-level rise are likely to increase C-3 abundance in Atlantic and Gulf coast marshes, investigations that quantify how patterns of C-3 and C-4 below ground biomass respond to environmental and biological factors stand to improve our understanding of ecosystem-wide impacts of global changes on coastal wetlands. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Saunders, CJ (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM saunders@fiu.edu RI Reynolds, James/G-6364-2010 NR 53 TC 16 Z9 20 U1 3 U2 23 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X J9 PLANT SOIL JI Plant Soil PD FEB PY 2006 VL 280 IS 1-2 BP 305 EP 322 DI 10.1007/s11104-005-3275-3 PG 18 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA 015UF UT WOS:000235575900028 ER PT J AU Hagedorn, M AF Hagedorn, M TI Avian genetic resource banking: Can fish embryos yield any clues for bird embryos? SO POULTRY SCIENCE LA English DT Article; Proceedings Paper CT 94th Annual Meeting of the Poultry-Science-Association CY JUL 31-AUG 03, 2005 CL Auburn Univ, Auburn, AL SP Poultry Sci Assoc HO Auburn Univ DE fish embryo; avian embryo; cryopreservation; genome resource banking; gonadal tissue ID BRACHYDANIO-RERIO; ZEBRAFISH EMBRYOS; OSMOMETRIC BEHAVIOR; PERMEABILITY; PRESERVATION; SENSITIVITY; SPERM; CELLS AB Cryopreservation of avian germplasm is becoming better understood and more commonly practiced. However, one area that would be of great benefit for genome resource banking is the preservation of avian embryos. Little is know about the cryobiology of avian embryos, and they have never been successfully cryopreserved. However, it is likely that they share many of the challenges of other yolk-filled multicompartmental embryos. For example, the fish embryo has 1) a large overall size, resulting in a low surface-to-volume ratio, which retards water and cryoprotectant efflux/influx; 2) large-sized cells, such as the yolk, which could increase the likelihood of membrane disruption by intracellular ice formation; 3) compartments, such as the blastoderm and yolk, with differing permeability properties; and 4) susceptibility to chilling injury. Both the avian and fish systems share many physical and anatomical properties, and it is predicted that some of the same permeability barriers would exist in both as well. Although the systems are similar, some of the goals, and thus the practices, to protect the genome may be quite different. One of these major goals in avian developmental biology is to produce chicken:chicken transgenic animals, especially those with germ line transmission. Producing efficient germ line transmissions and being able to cryopreserve these transmissions would be extremely beneficial to both basic and agricultural science. This could be accomplished through the cryopreservation of embryonic gonadal tissue followed by grafting into a host. The gonadal/tail-graft system would provide an advantage for cryopreservation because it is small (in comparison with the whole embryo), has fairly uniform tissue, and contains the essential primordial germ line cells capable of recreating the genetic line of interest. Moreover, because the chicken is such a robust model for most other avian species, the cryopreservation of the gonadal/tail-graft may potentially open up similar treatments for other commercially important species. C1 Smithsonian Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. RP Hagedorn, M (reprint author), Smithsonian Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. EM hagedornm@si.edu NR 32 TC 5 Z9 5 U1 0 U2 0 PU POULTRY SCIENCE ASSOC INC PI SAVOY PA 1111 N DUNLAP AVE, SAVOY, IL 61874-9604 USA SN 0032-5791 J9 POULTRY SCI JI Poult. Sci. PD FEB PY 2006 VL 85 IS 2 BP 251 EP 254 PG 4 WC Agriculture, Dairy & Animal Science SC Agriculture GA 008LS UT WOS:000235042800016 PM 16523623 ER PT J AU Neufeld, MJ AF Neufeld, MJ TI "Space superiority": Wernher von Braun's campaign for a nuclear-armed space station, 1946-1956 SO SPACE POLICY LA English DT Article AB The literature on the history of spaceflight has depicted the early 1950s Collier's articles mostly as a forerunner to the peaceful and scientific exploration of space. Yet the centerpiece of Wernher von Braun's plan was a manned space station that would serve as reconnaissance platform and orbiting battle station for achieving "space superiority" over the USSR. One its roles could be the launching of nuclear missiles. When challenged as to the station's defensibility, von Braun even posited pre-emptive atomic strikes from space as a response to the development of a hostile anti-satellite capability. (c) 2005 Smithsonian Institution. Published by Elsevier Ltd. All rights reserved. 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, MRC 311,POB 37012, Washington, DC 20560 USA. EM NeufeldM@si.edu NR 76 TC 7 Z9 7 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD FEB PY 2006 VL 22 IS 1 BP 52 EP 62 DI 10.1016/j.spacepol.2005.11.011 PG 11 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 016AS UT WOS:000235593500009 ER PT J AU Collins, AG Schuchert, P Marques, AC Jankowski, T Medina, M Schierwater, B AF Collins, AG Schuchert, P Marques, AC Jankowski, T Medina, M Schierwater, B TI Medusozoan phylogeny and character evolution clarified by new large and small subunit rDNA data and an assessment of the utility of phylogenetic mixture models SO SYSTEMATIC BIOLOGY LA English DT Article DE 18S; 28S; cubozoa; hydrozoa; medusa; molecular systematics; polyp; scyphozoa; staurozoa ID CARYBDEA-MARSUPIALIS LINNAEUS; CLASS-LEVEL RELATIONSHIPS; PHYLUM CNIDARIA; LIFE-CYCLE; ASTROHYDRA-JAPONICA; STRIATED-MUSCLE; TREE SELECTION; GENE SEQUENCE; GAP-JUNCTIONS; JELLYFISH AB A newly compiled data set of nearly complete sequences of the large subunit of the nuclear ribosome (LSU or 28S) sampled from 31 diverse medusozoans greatly clarifies the phylogenetic history of Cnidaria. These data have substantial power to discern among many of the competing hypotheses of relationship derived from prior work. Moreover, LSU data provide strong support at key nodes that were equivocal based on other molecular markers. Combining LSU sequences with those of the small subunit of the nuclear ribosome (SSU or 18S), we present a detailed working hypothesis of medusozoan relationships and discuss character evolution within this diverse clade. Stauromedusae, comprising the benthic, so-called stalked jellyfish, appears to be the sister group of all other medusozoans, implying that the free-swimming medusa stage, the motor nerve net, and statocysts of ecto-endodermal origin are features derived within Medusozoa. Cubozoans, which have had uncertain phylogenetic affinities since the elucidation of their life cycles, form a clade-named Acraspeda-with the scyphozoan groups Coronatae, Rhizostomeae, and Semaeostomeae. The polyps of both cubozoans and hydrozoans appear to be secondarily simplified. Hydrozoa is comprised by two well-supported clades, Trachylina and Hydroidolina. The position of Limnomedusae within Trachylina indicates that the ancestral hydrozoan had a biphasic life cycle and that the medusa was formed via an entocodon. Recently hypothesized homologies between the entocodon and bilaterian mesoderm are therefore suspect. Laingiomedusae, which has often been viewed as a close ally of the trachyline group Narcomedusae, is instead shown to be unambiguously a member of Hydroidolina. The important model organisms of the Hydra species complex are part of a clade, Aplanulata, with other hydrozoans possessing direct development not involving a ciliated planula stage. Finally, applying phylogenetic mixture models to our data proved to be of little additional value over a more traditional phylogenetic approach involving explicit hypothesis testing and bootstrap analyses under multiple optimality criteria. C1 NMFS, Natl Systemat Lab, Smithsonian Inst, Washington, DC 20013 USA. Museum Nat Hist, CH-1211 Geneva, Switzerland. Univ Sao Paulo, Dept Zool, Inst Biosci, Sao Paulo, Brazil. ETH, EAWAG, W&T, Swiss Fed Inst Aquat Sci & Technol, CH-8600 Dubendorf, Switzerland. DOE Joint Genome Inst, Walnut Creek, CA 94598 USA. ITZ, TiHo Hannover, D-30559 Hannover, Germany. RP Collins, AG (reprint author), NMFS, Natl Systemat Lab, Smithsonian Inst, MRC-153,POB 37012, Washington, DC 20013 USA. EM CollinsA@SI.edu RI Collins, Allen/A-7944-2008; Marques, Antonio/E-8049-2011 OI Collins, Allen/0000-0002-3664-9691; Marques, Antonio/0000-0002-2884-0541 NR 94 TC 190 Z9 199 U1 2 U2 26 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD FEB PY 2006 VL 55 IS 1 BP 97 EP 115 DI 10.1080/10635150500433615 PG 19 WC Evolutionary Biology SC Evolutionary Biology GA 016LW UT WOS:000235622700008 PM 16507527 ER PT J AU De Queiroz, K AF De Queiroz, K TI The PhyloCode and the distinction between taxonomy and nomenclature SO SYSTEMATIC BIOLOGY LA English DT Editorial Material ID PHYLOGENETIC DEFINITIONS; RANKS C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. RP De Queiroz, K (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. EM dequeirk@si.edu NR 13 TC 27 Z9 30 U1 1 U2 7 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD FEB PY 2006 VL 55 IS 1 BP 160 EP 162 DI 10.1080/10635150500431221 PG 4 WC Evolutionary Biology SC Evolutionary Biology GA 016LW UT WOS:000235622700014 ER PT J AU Boxshall, GA Strong, EE AF Boxshall, GA Strong, EE TI An extraordinary shift in life habit within a genus of cyclopid copepods in Lake Tanganyika SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE anatomy; Cyclopoida; ectoparasite; endemic; first record from nonampullariid ID EAST-AFRICA; FRESH-WATER; PHYLOGENETIC-RELATIONSHIPS; PARAERGASILUS-RYLOVI; CRUSTACEA; ZOOPLANKTON; GASTROPODS; OSTRACODA; IDENTITY; FISHES AB We here describe a new species of cyclopid copepod, Eucyclops bathanalicola sp. nov., parasitic on a gastropod endemic to Lake Tanganyika, Bathanalia straeleni (Cerithioidea, Paludomidae). E. bathanalicola is distinguished by the possession of praecoxal claws on the maxillules, by the modified maxillae which lack any trace of an endopod on the powerful distal claw, and by the reduction of the maxillipeds to minute unarmed lobes. In the character states exhibited by the female body, antennules and swimming legs 1-5, the new species closely resembles a typical free living Eucyclops. The impact of the adoption of parasitism as a life habit is expressed primarily in the modification of the postmandibular mouthparts. As a member of the Cyclopidae, this species represents a unique foray into a parasitic lifestyle from an otherwise free-living group of copepods inhabiting Lake Tanganyika. This is the first record of a parasitic copepod on a mollusc host within this ancient lake and only the second family of freshwater gastropods reported to host copepods. (c) 2006 The Linnean Society of London. C1 Nat Hist Museum, Dept Zool, London SW7 5BD, England. Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Boxshall, GA (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM g.boxshall@nhm.ac.uk OI Boxshall, Geoffrey/0000-0001-8170-7734 NR 59 TC 10 Z9 10 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD FEB PY 2006 VL 146 IS 2 BP 275 EP 285 DI 10.1111/j.1096-3642.2006.00206.x PG 11 WC Zoology SC Zoology GA 010DY UT WOS:000235168300007 ER PT J AU Hunt, G Roy, K AF Hunt, G Roy, K TI Climate change, body size evolution, and Cope's Rule in deep-sea ostracodes SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Bergmann's Rule; Ostracoda; temperature ID LIFE-HISTORY PUZZLE; BERGMANNS RULE; LIKELIHOOD APPROACH; TEMPERATURE-CHANGE; GROWTH-RATE; ECTOTHERMS; PATTERNS; MAMMALS; EXPLANATION; TRENDS AB Causes of macroevolutionary trends in body size, such as Cope's Rule, the tendency of body size to increase over time, remain poorly understood. We used size measurements from Cenozoic populations of the ostracode genus Poseidonamicus, in conjunction with phylogeny and paleotemperature estimates, to show that climatic cooling leads to significant increases in body size, both overall and within individual lineages. The magnitude of size increase due to Cenozoic cooling is consistent with temperature-size relationships in geographically separated modern populations (Bergmann's Rule). Thus population-level phenotypic evolution in response to climate change can be an important determinant of macroevolutionary trends in body size. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. RP Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM hunte@si.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 NR 58 TC 92 Z9 94 U1 0 U2 30 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 31 PY 2006 VL 103 IS 5 BP 1347 EP 1352 DI 10.1073/pnas.0510550103 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 009EO UT WOS:000235094300036 PM 16432187 ER PT J AU Lorenzo, M Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J AF Lorenzo, M Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J TI Muriceanol, a 24(28)-epoxide sterol link in the carbon flux toward side-chain dealkylation of sterols SO EUROPEAN JOURNAL OF ORGANIC CHEMISTRY LA English DT Article DE octocoral; non-zooxanthellate gorgonia; Muricea spp; 24(28)-epoxisterol; side-chain dealkylation; pregnanes; biogenesis ID BIOSYNTHESIS; CHOLESTEROL; PHYTOSTEROLS; EPOXIDE; ORIGIN AB Side-chain-oxidized C-28-sterol 1 and one new pregnane metabolite 2 were isolated from eastern Pacific Muricea spp. The C-24(28)-epoxide functionality is a key intermediate in the C-24-dealkylation mechanism of the conversion of phytosterol to cholesterol by phytophagous insects. Certain marine invertebrates share this dealkylation pathway; however, such a key epoxide feature has not yet been found in a naturally occurring sterol from marine invertebrates. The unusual oxidation pattern of the side chain of I encourages speculation about its biogenesis and converts this non-zooxanthellate gorgonia into an interesting candidate organism for biosynthetic studies on C-24-dealkylation of phytosterols in octocorals. The (22S)-22-hydroxy group, after 24-dealkylation of 1, may be an advantageous functionalization in the side-chain cleavage to C-21-pregnane steroids in Muricea spp. ((c) Wiley-VCH Verlag GmbH & Co. KGaA, 69451 Weinheim, Germany, 2006) C1 CSIC, Inst Prod Nat & Agrobiol, San Cristobal la Laguna 38206, Tenerife, Spain. Univ Magallanes, Ctr Estudios Cuaternario, Fac Ciencias, Dept Quim, Punta Arenas, Chile. Univ Panama, Dept Biol Marina & Limnol, Panama City, Panama. Smithsonian Trop Res Inst, Balboa, Panama. Univ Chile, Fac Ciencias, Dept Quim, Santiago, Chile. RP Darias, J (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez 3,Apdo 195, San Cristobal la Laguna 38206, Tenerife, Spain. EM jdarias@ipna.csic.es RI Cueto, MERCEDES/L-3185-2014 OI Cueto, MERCEDES/0000-0002-9112-6877 NR 17 TC 11 Z9 11 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1434-193X J9 EUR J ORG CHEM JI Eur. J. Org. Chem. PD JAN 30 PY 2006 IS 3 BP 582 EP 585 DI 10.1002/ejoc.200500775 PG 4 WC Chemistry, Organic SC Chemistry GA 012OR UT WOS:000235349000003 ER PT J AU Liu, X Chance, K Sioris, CE Kurosu, TP Spurr, RJD Martin, RV Fu, TM Logan, JA Jacob, DJ Palmer, PI Newchurch, MJ Megretskaia, IA Chatfield, RB AF Liu, X Chance, K Sioris, CE Kurosu, TP Spurr, RJD Martin, RV Fu, TM Logan, JA Jacob, DJ Palmer, PI Newchurch, MJ Megretskaia, IA Chatfield, RB TI First directly retrieved global distribution of tropospheric column ozone from GOME: Comparison with the GEOS-CHEM model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MODIFIED-RESIDUAL METHOD; MOZAIC AIRBORNE PROGRAM; IN-SERVICE AIRCRAFT; 1997-1998 EL-NINO; SATELLITE MEASUREMENTS; MAPPING SPECTROMETER; TOMS MEASUREMENTS; UNITED-STATES; SURFACE OZONE; WATER-VAPOR AB [1] We present the first directly retrieved global distribution of tropospheric column ozone from Global Ozone Monitoring Experiment (GOME) ultraviolet measurements during December 1996 to November 1997. The retrievals clearly show signals due to convection, biomass burning, stratospheric influence, pollution, and transport. They are capable of capturing the spatiotemporal evolution of tropospheric column ozone in response to regional or short time-scale events such as the 1997 - 1998 El Nino event and a 10 - 20 DU change within a few days. The global distribution of tropospheric column ozone displays the well-known wave-1 pattern in the tropics, nearly zonal bands of enhanced tropospheric column ozone of 36 - 48 DU at 20 degrees S-30 degrees S during the austral spring and at 25 degrees N - 45 degrees N during the boreal spring and summer, low tropospheric column ozone of < 30 DU uniformly distributed south of 35 degrees S during all seasons, and relatively high tropospheric column ozone of > 33 DU at some northern high-latitudes during the spring. Simulation from a chemical transport model corroborates most of the above structures, with small biases of < +/- 5 DU and consistent seasonal cycles in most regions, especially in the southern hemisphere. However, significant positive biases of 5 - 20 DU occur in some northern tropical and subtropical regions such as the Middle East during summer. Comparison of GOME with monthly-averaged Measurement of Ozone and Water Vapor by Airbus in-service Aircraft (MOZAIC) tropospheric column ozone for these regions usually shows good consistency within 1 sigma standard deviations and retrieval uncertainties. Some biases can be accounted for by inadequate sensitivity to lower tropospheric ozone, the different spatiotemporal sampling and the spatiotemporal variations in tropospheric column ozone. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Atmospher Chem & Dynam Branch, Moffett Field, CA 94035 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. RP Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM xliu@cfa.harvard.edu RI Chem, GEOS/C-5595-2014; Martin, Randall/C-1205-2014; Palmer, Paul/F-7008-2010; Liu, Xiong/P-7186-2014; Fu, Tzung-May/N-3418-2015; Martin, Randall/A-2051-2008; OI Sioris, Christopher/0000-0003-1168-8755; Martin, Randall/0000-0003-2632-8402; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 NR 77 TC 65 Z9 66 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 28 PY 2006 VL 111 IS D2 AR D02308 DI 10.1029/2005JD006564 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 008FY UT WOS:000235026800007 ER PT J AU Raven, P Fauquet, C Swaminathan, MS Borlaug, N Samper, C AF Raven, P Fauquet, C Swaminathan, MS Borlaug, N Samper, C TI Where next for genome sequencing? SO SCIENCE LA English DT Letter C1 Missouri Bot Garden, St Louis, MO 63110 USA. Danforth Plant Sci Ctr, St Louis, MO 63132 USA. MS Swaminathan Res Fdn, Madras, Tamil Nadu, India. Texas A&M Univ, College Stn, TX 77843 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Raven, P (reprint author), Missouri Bot Garden, 2345 Tower Grove Ave,POB 299, St Louis, MO 63110 USA. NR 0 TC 8 Z9 8 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 JAN 27 PY 2006 VL 311 IS 5760 BP 468 EP 468 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 008WM UT WOS:000235071400018 PM 16439644 ER PT J AU Behrensmeyer, AK AF Behrensmeyer, AK TI Climate change and human evolution SO SCIENCE LA English DT Editorial Material ID AFRICAN CLIMATE; HOMININ EVOLUTION; VEGETATION; RECORDS; ORIGIN; HOMO C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Behrensmeyer, AK (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM behrensa@si.edu NR 32 TC 70 Z9 75 U1 1 U2 43 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 JAN 27 PY 2006 VL 311 IS 5760 BP 476 EP 478 DI 10.1126/science.1116051 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 008WM UT WOS:000235071400032 PM 16439650 ER PT J AU Wills, C Harms, KE Condit, R King, D Thompson, J He, FL Muller-Landau, HC Ashton, P Losos, E Comita, L Hubbell, S LaFrankie, J Bunyavejchewin, S Dattaraja, HS Davies, S Esufali, S Foster, R Gunatilleke, N Gunatilleke, S Hall, P Itoh, A John, R Kiratiprayoon, S de Lao, SL Massa, M Nath, C Noor, MNS Kassim, AR Sukumar, R Suresh, HS Sun, IF Tan, S Yamakura, T Zimmerman, E AF Wills, C Harms, KE Condit, R King, D Thompson, J He, FL Muller-Landau, HC Ashton, P Losos, E Comita, L Hubbell, S LaFrankie, J Bunyavejchewin, S Dattaraja, HS Davies, S Esufali, S Foster, R Gunatilleke, N Gunatilleke, S Hall, P Itoh, A John, R Kiratiprayoon, S de Lao, SL Massa, M Nath, C Noor, MNS Kassim, AR Sukumar, R Suresh, HS Sun, IF Tan, S Yamakura, T Zimmerman, E TI Nonrandom processes maintain diversity in tropical forests SO SCIENCE LA English DT Article ID POPULATION REGULATION; DENSITY-DEPENDENCE; NEOTROPICAL FOREST; SPATIAL-PATTERNS; SOIL PATHOGENS; RAIN-FORESTS; TREE; PRODUCTIVITY; MAINTENANCE; MORTALITY AB An ecological community's species diversity tends to erode through time as a result of stochastic extinction, competitive exclusion, and unstable host-enemy dynamics. This erosion of diversity can be prevented over the short term if recruits are highly diverse as a result of preferential recruitment of rare species or, alternatively, if rare species survive preferentially, which increases diversity as the ages of the individuals increase. Here, we present census data from seven New and Old World tropical forest dynamics plots that all show the latter pattern. Within local areas, the trees that survived were as a group more diverse than those that were recruited or those that died. The larger (and therefore on average older) survivors were more diverse within local areas than the smaller survivors. When species were rare in a local area, they had a higher survival rate than when they were common, resulting in enrichment for rare species and increasing diversity with age and size class in these complex ecosystems. C1 Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Harvard Univ, Herbaria, Arnold Arboretum Asia Program, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00931 USA. Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA. Univ Georgia, Dept Plant Sci, Athens, GA 30602 USA. Nanyang Technol Univ, Natl Inst Educ, Arnold Arboretum Asia Program, Ctr Trop Forest Sci, Singapore 637616, Singapore. Thai Natl Pk Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India. Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Florida State Univ, Dept Biol, Tallahassee, FL 32309 USA. Osaka City Univ, Fac Sci, Plant Ecol Lab, Sumiyoshi Ku, Osaka 558, Japan. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. Forest Res Inst Malaysia, Forest Environm Div, Kuala Lumpur 52109, Malaysia. Tunghai Univ, Ctr Trop Ecol & Biodivers, Taipei 407, Taiwan. Sarawak Forest Dept, Forest Res Ctr, Kuching 93250, Sarawak, Malaysia. RP Wills, C (reprint author), Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. EM cwills@ucsd.edu RI Thompson, Jill/K-2200-2012; Raman, Sukumar/C-9809-2013; OI Thompson, Jill/0000-0002-4370-2593; Comita, Liza/0000-0002-9169-1331 NR 28 TC 109 Z9 117 U1 4 U2 84 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 JAN 27 PY 2006 VL 311 IS 5760 BP 527 EP 531 DI 10.1126/science.1117715 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 008WM UT WOS:000235071400047 PM 16439661 ER PT J AU Hajibabaei, M Janzen, DH Burns, JM Hallwachs, W Hebert, PDN AF Hajibabaei, M Janzen, DH Burns, JM Hallwachs, W Hebert, PDN TI DNA barcodes distinguish species of tropical Lepidoptera SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Area de Conservacion Guanacaste; cytochrome c oxidase; Hesperiidae; Sphingidae; Saturniidae ID SEQUENCE ALIGNMENT; CLASSIFICATION; BIODIVERSITY; SYSTEMATICS; BIOLOGY; RATES; LIFE AB Although central to much biological research, the identification of species is often difficult. The use of DNA barcodes, short DNA sequences from a standardized region of the genome, has recently been proposed as a tool to facilitate species identification and discovery. However, the effectiveness of DNA barcoding for identifying specimens in species-rich tropical biotas is unknown. Here we show that cytochrome c oxidase I DNA barcodes effectively discriminate among species in three Lepidoptera families from Area de Conservacion Guanacaste in northwestern Costa Rica. We found that 97.9% of the 521 species recognized by prior taxonomic work possess distinctive cytochrome c oxidase I barcodes and that the few instances of interspecific sequence overlap involve very similar species. We also found two or more barcode clusters within each of 13 supposedly single species. Covariation between these clusters and morphological and/or ecological traits indicates overlooked species complexes. if these results are general, DNA barcoding will significantly aid species identification and discovery in tropical settings. C1 Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Hajibabaei, M (reprint author), Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. EM mhajibab@uoguelph.ca; djanzen@sas.upenn.edu RI Hebert, Paul/C-4161-2013 OI Hebert, Paul/0000-0002-3081-6700 NR 23 TC 639 Z9 756 U1 16 U2 132 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 24 PY 2006 VL 103 IS 4 BP 968 EP 971 DI 10.1073/pnas.0510466103 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 007AC UT WOS:000234938300025 PM 16418261 ER PT J AU Furlanetto, SR Zaldarriaga, M Hernquist, L AF Furlanetto, SR Zaldarriaga, M Hernquist, L TI The effects of reionization on Ly alpha galaxy surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : evolution; intergalactic medium; cosmology : theory ID GUNN-PETERSON TROUGH; LYMAN-BREAK GALAXIES; PROBE WMAP OBSERVATIONS; DARK-MATTER HALOES; HIGH-REDSHIFT; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; STAR-FORMATION; NEUTRAL HYDROGEN; STELLAR SOURCES AB Searches for Ly alpha emission lines are among the most effective ways to identify high-redshift galaxies. They are particularly interesting because they probe not only the galaxies themselves but also the ionization state of the intergalactic medium: nearby neutral gas efficiently absorbs Ly alpha photons. The observed linestrengths depend on the amount by which each photon is able to redshift away from line centre before encountering neutral gas and hence on the size distribution of HII regions surrounding the sources. Here, we use an analytic model of that size distribution to study the effects of reionization on the luminosity function of Ly alpha emitters and their observed spatial distribution. Our model includes the clustering of high-redshift galaxies and thus contains ionized bubbles much larger than those expected around isolated galaxies. As a result, Ly alpha-emitting galaxies remain visible earlier in reionization: we expect the number counts to decline by only a factor of similar to 2 ( or 10) when the mean ionized fraction falls to (x) over bar (i) similar to 0.75 (or 0.5) in the simplest model. Moreover, the absorption is not uniform across the sky: galaxies remain visible only if they sit inside large bubbles, which become increasingly rare as (x) over bar (i) decreases. Thus, the size distribution also affects the apparent clustering of Ly alpha-selected galaxies. On large scales, it traces that of the large bubbles, which in our model are more biased than the galaxies. On small scales, the clustering increases rapidly as (x) over bar (i) decreases because large HII regions surround strong galaxy overdensities, so a survey automatically selects only those galaxies with neighbours. The transition between these two regimes occurs at the characteristic bubble size. Hence, large Ly alpha galaxy surveys have the potential to measure directly the size distribution of HII regions during reionization. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP CALTECH, Div Phys Math & Astron, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu NR 59 TC 80 Z9 80 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 21 PY 2006 VL 365 IS 3 BP 1012 EP 1020 DI 10.1111/j.1365-2966.2005.09785.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VV UT WOS:000234853600028 ER PT J AU Landt, H Perlman, ES Padovani, P AF Landt, H Perlman, ES Padovani, P TI VLA observations of a new population of blazars SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : general; galaxies : active; quasars : general; radio continuum : galaxies ID BL-LACERTAE OBJECTS; SPECTRUM RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; X-RAY-PROPERTIES; COMPLETE SAMPLE; OPTICAL SPECTROSCOPY; ENERGY-DISTRIBUTIONS; STEEP-SPECTRUM; LOUD QUASARS; LAC OBJECTS AB We present the first deep VLA radio images of flat-spectrum radio quasars (FSRQs) with multiwavelength emission properties similar to those of BL Lacertae (BL Lac) objects with synchrotron X-rays. Our observations of 25 of these sources show that their radio morphologies are similar to those of other radio quasars. However, their range of extended powers is more similar to that of BL Lac objects and extends down to the low values typical of FR I radio galaxies. Five out of our nine lobe-dominated sources have extended radio powers in the range typical of both FR I and FR II radio galaxies, but their extended radio structure is clearly FR II-like. Therefore, we have not yet found a large population of radio quasars hosted by FR I galaxies. Two-thirds of our sources have a core-dominated radio morphology and thus X-rays likely dominated by the jet. We find that their ratios of radio core to total X-ray luminosity are low and in the regime indicative of synchrotron X-rays. This result shows that also blazars with strong emission lines can produce jets of high-energy synchrotron emission, and it undermines at least in part the "blazar sequence'' scenario, which advocates the position that particle Compton cooling by an external radiation field governs the frequency of the synchrotron emission peak. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. European So Observ, D-85748 Garching, Germany. RP Landt, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Padovani, Paolo/0000-0002-4707-6841; Perlman, Eric/0000-0002-3099-1664 NR 60 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 JAN 20 PY 2006 VL 637 IS 1 BP 183 EP 199 DI 10.1086/498261 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RT UT WOS:000235130800017 ER PT J AU Jonsson, P Cox, TJ Primack, JR Somerville, RS AF Jonsson, P Cox, TJ Primack, JR Somerville, RS TI Simulations of dust in interacting galaxies. I. Dust attenuation SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : interactions; galaxies : starburst; methods : numerical; radiative transfer ID PARTICLE HYDRODYNAMICS SIMULATIONS; SPECTRAL ENERGY-DISTRIBUTION; DISK DOMINATED GALAXIES; BAND SURFACE PHOTOMETRY; STAR-FORMATION RATE; DIGITAL SKY SURVEY; SPIRAL GALAXIES; STARBURST GALAXIES; INFRARED GALAXIES; MAJOR MERGERS AB A new Monte Carlo radiative transfer code, SUNRISE, is used in conjunction with hydrodynamic simulations of major galaxy mergers to calculate the effects of dust in such systems. Dust has a profound effect on the emerging radiation, consistent with observations of dust absorption in starburst galaxies. The dust attenuation increases with luminosity such that at peak luminosities similar to 90% of the bolometric luminosity is absorbed by dust. We find that our predictions agree with observed relationships between the UV spectral slope and the fraction of light absorbed by dust (IRX-beta) and observational estimates of the optical depth as a function of intrinsic B-band or UV luminosity. In general, the detailed appearance of the merging event depends on the stage of the merger and the geometry of the encounter. The fraction of bolometric energy absorbed by the dust, however, is a robust quantity that can be predicted from the intrinsic properties bolometric luminosity, baryonic mass, star formation rate, and metallicity of the simulated system. This paper presents fitting formulae, valid over a wide range of masses and metallicities, from which the absorbed fraction of luminosity ( and consequently also the infrared dust luminosity) can be predicted. The attenuation of the luminosity at specific wavelengths can also be predicted, albeit with a larger scatter due to the variation with viewing angle. These formulae for dust attenuation are consistent with earlier studies and would be suitable for inclusion in theoretical models, e. g., semianalytic models, of galaxy formation and evolution. C1 Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Jonsson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM patrik@ucolick.org; tcox@cfa.harvard.edu; joel@scipp.ucsc.edu; rachel@mpia-hd.mpg.de NR 80 TC 60 Z9 60 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 JAN 20 PY 2006 VL 637 IS 1 BP 255 EP 268 DI 10.1086/497567 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RT UT WOS:000235130800022 ER PT J AU Cordes, JM Freire, PCC Lorimer, DR Camilo, F Champion, DJ Nice, DJ Ramachandran, R Hessels, JWT Vlemmings, W van Leeuwen, J Ransom, SM Bhat, NDR Arzoumanian, Z McLaughlin, MA Kaspi, VM Kasian, L Deneva, JS Reid, B Chatterjee, S Han, JL Backer, DC Stairs, IH Deshpande, AA Faucher-Giguere, CA AF Cordes, JM Freire, PCC Lorimer, DR Camilo, F Champion, DJ Nice, DJ Ramachandran, R Hessels, JWT Vlemmings, W van Leeuwen, J Ransom, SM Bhat, NDR Arzoumanian, Z McLaughlin, MA Kaspi, VM Kasian, L Deneva, JS Reid, B Chatterjee, S Han, JL Backer, DC Stairs, IH Deshpande, AA Faucher-Giguere, CA TI Arecibo pulsar survey using alfa. I. Survey strategy and first discoveries SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; pulsars : individual (PSR J0628+09,PSR J1906+07; PSR J1928+1746); surveys ID HIGH-FREQUENCY SURVEY; BLACK-HOLE BINARIES; GAMMA-RAY SOURCES; GALACTIC PLANE; YOUNG PULSARS; RADIO PULSARS; RADIATION; SEARCHES; CATALOG; SYSTEMS AB We report results from the initial stage of a long-term pulsar survey of the Galactic plane using the Arecibo L-band Feed Array (ALFA), a seven-beam receiver operating at 1.4 GHz with 0.3 GHz bandwidth, and fast-dump digital spectrometers. The search targets lowGalactic latitudes, vertical bar b vertical bar greater than or similar to 5 degrees, in the accessible longitude ranges 32 degrees greater than or similar to l greater than or similar to 77 degrees and 168 degrees less than or similar to l less than or similar to 214 degrees. The instrumentation, data processing, initial survey observations, sensitivity, and database management are described. Data discussed here were collected over a 100 MHz passband centered on 1.42 GHz using a spectrometer that recorded 256 channels every 64 mu s. Analysis of the data with their full time and frequency resolutions is ongoing. Here we report the results of a preliminary, low-resolution analysis for which the data were decimated to speed up the processing. We have detected 29 previously known pulsars and discovered 11 new ones. One of these, PSR J1928+ 1746, with a period of 69 ms and a relatively low characteristic age of 82 kyr, is a plausible candidate for association with the unidentified EGRETsource 3EG J1928+1733. Another, PSR J1906+07, is a nonrecycled pulsar in a relativistic binary with an orbital period of 3.98 hr. In parallel with the periodicity analysis, we also search the data for isolated dispersed pulses. This technique has resulted in the discovery of PSR J0628+09, an extremely sporadic radio emitter with a spin period of 1.2s. Simulations we have carried out indicate that similar to 1000 new pulsars will be found in our ALFA survey. In addition to providing a large sample for use in population analyses and for probing the magnetoionic interstellar medium, the survey maximizes the chances of finding rapidly spinning millisecond pulsars and pulsars in compact binary systems. Our search algorithms exploit the multiple data streams from ALFA to discriminate between radio frequency interference and celestial signals, including pulsars and possibly new classes of transient radio sources. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Cornell Univ, NAIC, Ithaca, NY 14853 USA. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Columbia Univ, Astrophys Lab, New York, NY 10027 USA. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. MIT, Haystack Observ, Westford, MA 01886 USA. Univ Space Res Assoc, EUD, NASA, Code 662, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Cordes, JM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RI Deshpande, Avinash/D-4868-2012; Astronomy & Astrophysics Group, Raman Res Institute/D-4046-2012; Bhat, Ramesh/B-7396-2013; OI Nice, David/0000-0002-6709-2566; Ransom, Scott/0000-0001-5799-9714; /0000-0002-2700-9916 NR 46 TC 98 Z9 101 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 JAN 20 PY 2006 VL 637 IS 1 BP 446 EP 455 DI 10.1086/498335 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RT UT WOS:000235130800039 ER PT J AU Camilo, F Ransom, SM Gaensler, BM Slane, PO Lorimer, DR Reynolds, J Manchester, RN Murray, SS AF Camilo, F Ransom, SM Gaensler, BM Slane, PO Lorimer, DR Reynolds, J Manchester, RN Murray, SS TI PSR J1833-1034: Discovery of the central young pulsar in the supernova remnant G21.5-0.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G21.5-0.9); pulsars : individual (PSR J1833-1034); stars : neutron; supernova remnants ID GREEN-BANK-TELESCOPE; GALACTIC PLANE SURVEY; X-RAY OBSERVATIONS; RADIO PULSARS; WIND NEBULAE; CRAB-NEBULA; MILLISECOND PULSAR; MOLECULAR CLOUDS; SNR G21.5-0.9; PROPER-MOTION AB We have discovered the pulsar associated with the supernova remnant G21.5-0.9. PSR J1833-1034, with spin period P = 61.8 ms and dispersion measure 169 cm(-3) pc, is very faint, with pulse-averaged flux density of approximate to 70 mu Jy at a frequency of 1.4 GHz, and was first detected in a deep search with the Parkes telescope. Subsequent observations with Parkes and the Green Bank Telescope have confirmed this detection and yield a period derivative. P 2.02 x 10(-13). These spin parameters imply a characteristic age tau(c) = 4.8 kyr and a spin-down luminosity E 3: 3; 10(37) ergs s(-1), the latter value exceeded only by the Crab pulsar among the rotation-powered pulsars known in our Galaxy. The pulsar has an unusually steep radio spectrum in the 0.8-2.0 GHz range, with power-law index approximate to 3.0, and a narrow single-peaked pulse profile with FWHM of 0.04P. We have analyzed 350 ks of archival Chandra X-Ray Observatory HRC data and find a pointlike source of luminosity approximate to 3 x 10(-5). E, offset from the center of an elliptical region of size approximate to 70"5" and luminosity approximate to 10(-3). E within which likely lies the pulsar wind termination shock. We have searched for X-ray pulsations in a 30 ks HRC observation without success, deriving a pulsed fraction upper limit for a sinusoidal pulse shape of about 70% of the pulsar flux. We revisit the distance to G21.5-0.9 based on H (I) and CO observations, arguing that it is 4.7 +/- 0.4 kpc. We use existing X-ray and radio observations of the pulsar wind nebula, along with the measured properties of its engine and a recent detection of the supernova remnant shell, to argue that G21.5-0.9 and PSR J1833-1034 are much younger than tau(c) and likely their true age is <= 1000 yr. In that case, the initial spin period of the pulsar was >= 55 ms. C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Parkes, NSW 2870, Australia. Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA. RI Gaensler, Bryan/F-8655-2010; OI Ransom, Scott/0000-0001-5799-9714; Gaensler, Bryan/0000-0002-3382-9558 NR 89 TC 55 Z9 55 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 JAN 20 PY 2006 VL 637 IS 1 BP 456 EP 465 DI 10.1086/498386 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RT UT WOS:000235130800040 ER PT J AU Williams, BF Garcia, MR McClintock, JE Primini, FA Murray, SS AF Williams, BF Garcia, MR McClintock, JE Primini, FA Murray, SS TI A soft X-ray transient in the M31 bulge SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : individual (M31); X-rays : binaries; X-rays : stars ID RXTE SPECTRAL OBSERVATIONS; BLACK-HOLE; TIMING EVOLUTION; CENTRAL REGION; XMM-NEWTON; OUTBURST; CHANDRA; NOVA; BINARIES AB We have examined a probable soft X-ray transient source in the M31 bulge at R: A: 0h42m41.(s)814 +/- 0."08, decl: 41 degrees 16'35."86 +/- 0."07. On the three occasions we observed the source, its spectrum was soft (kT(in) approximate to 1 keV). The brightest detection of the source was on 2004 July 17, with a 0.3-7 keV luminosity of similar to 5 x 10(37) ergs s(-1). The only previous detection of the source was in 1979 by the Einstein observatory. The multiple detections over 25 years suggest that the duty cycle of the source is in the range 0.02-0.06. Coordinated HSTACS imaging before, during, and after the outburst revealed no variable optical source within the position errors of the X-ray source. The optical data place a firm upper limit on the brightness of the counterpart of the X-ray outburst of B > 24.7, suggesting that the binary has a period <= 5.2 days. The X-ray spectrum and lack of bright stars at the source location indicate that the source was a soft transient event occurring in a low-mass X-ray binary, making this source a good black hole candidate in M31. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; garcia@head.cfa.harvard.edu; jem@head.cfa.harvard.edu; fap@head.cfa.harvard.edu; ssm@head.cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 28 TC 6 Z9 6 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 JAN 20 PY 2006 VL 637 IS 1 BP 479 EP 485 DI 10.1086/498297 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RT UT WOS:000235130800042 ER PT J AU Haverkorn, M Gaensler, BM Brown, JC Bizunok, NS McClure-Griffiths, NM Dickey, JM Green, AJ AF Haverkorn, M Gaensler, BM Brown, JC Bizunok, NS McClure-Griffiths, NM Dickey, JM Green, AJ TI Enhanced small-scale faraday rotation in the galactic spiral arms SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : magnetic fields; ISM : structure; radio continuum : ISM; techniques : polarimetric; turbulence ID DENSITY POWER SPECTRUM; MAGNETOHYDRODYNAMIC TURBULENCE; INTERSTELLAR-MEDIUM; INNER GALAXY; PLANE SURVEY; SIMULATIONS AB We present an analysis of the rotation measures (RMs) of polarized extragalactic point sources in the Southern Galactic Plane Survey. This work demonstrates that the statistics of fluctuations in RM differ for the spiral arms and the interarm regions. Structure functions of RM are flat in the spiral arms, while they increase in the interarms. This indicates that there are no correlated RM fluctuations in the magnetoionized interstellar medium in the spiral arms on scales larger than similar to 0.degrees 5, corresponding to similar to 17 pc in the nearest spiral arm probed. The nonzero slopes in interarm regions imply a much larger scale of RM fluctuations. We conclude that fluctuations in the magnetoionic medium in the Milky Way spiral arms are not dominated by the mainly supernova-driven turbulent cascade in the global ISM but are probably due to a different source, most likely H II regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. Australia Telescope Natl Facil, CSIRO, Epping, NSW 1710, Australia. Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Haverkorn, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM mhaverkorn@cfa.harvard.edu; bgaensler@cfa.harvard.edu; jocat@ras.ucalgary.ca; nbizunok@cfa.harvard.edu; naomi.mcclure-griffiths@csiro.au; john.dickey@utas.edu.au; agreen@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 25 TC 51 Z9 51 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 JAN 20 PY 2006 VL 637 IS 1 BP L33 EP L35 DI 10.1086/500543 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RW UT WOS:000235131100009 ER PT J AU Matthews, LD Karovska, M AF Matthews, LD Karovska, M TI First resolved images of the Mira AB symbiotic binary at centimeter wavelengths SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; radio continuum : stars; stars : AGB and post-AGB; stars : individual (Mira AB); stars : winds, outflows ID HUBBLE-SPACE-TELESCOPE; X-RAYS; STARS; EMISSION; RADIO; ACCRETION; SPECTRUM; SYSTEM; WINDS; CETI AB We report the first spatially resolved radio continuum measurements of the Mira AB symbiotic binary system, based on observations obtained with the Very Large Array (VLA). This is the first time that a symbiotic binary has been resolved unambiguously at centimeter wavelengths. We describe the results of VLA monitoring of both stars over a 10 month period, together with constraints on their individual spectral energy distributions, variability, and radio emission mechanisms. The emission from Mira A is consistent with originating from a radio photosphere, while the emission from Mira B appears best explained as free-free emission from an ionized circumstellar region similar to(1-10) x 10(13) cm in radius. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 23 Z9 23 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 JAN 20 PY 2006 VL 637 IS 1 BP L49 EP L52 DI 10.1086/500303 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RW UT WOS:000235131100013 ER PT J AU Risaliti, G Sani, E Maiolino, R Marconi, A Berta, S Braito, V Della Ceca, R Franceschini, A Salvati, M AF Risaliti, G Sani, E Maiolino, R Marconi, A Berta, S Braito, V Della Ceca, R Franceschini, A Salvati, M TI The double active galactic nucleus in NGC 6240 revealed through 3-5 mu m spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 6240) ID NGC 6240; GALAXIES; DUST AB We present 3-5 mu m spectroscopy of the interacting system NGC 6240, revealing the presence of two active galactic nuclei (AGNs). The brightest (southern) nucleus shows up with a starburst-like emission, with a prominent 3.3 mu m emission feature. However, the presence of an AGN is revealed by the detection of a broad Bra emission line, with a width of similar to 1800 km s(-1). The spectrum of the faintest (northern) nucleus shows typical AGN features, such as a steep continuum and broad absorption features in the M band. We discuss the physical properties of the dusty absorbers/emitters, and we show that in both nuclei, the AGN is dominant in the 3-5 mu m band but that its contribution to the total luminosity is small (a few percent of the starburst emission). C1 INAF, Osserv Arceti, Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. INAF, Osserv Astron Brera, I-20121 Milan, Italy. RP Risaliti, G (reprint author), INAF, Osserv Arceti, Largo E Fermi 5, Florence, Italy. EM grisaliti@cfa.harvard.edu RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X NR 18 TC 15 Z9 15 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 JAN 20 PY 2006 VL 637 IS 1 BP L17 EP L20 DI 10.1086/500588 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RW UT WOS:000235131100005 ER PT J AU McCoy, TJ Carlson, WD Nittler, LR Stroud, RM Bogard, DD Garrison, DH AF McCoy, TJ Carlson, WD Nittler, LR Stroud, RM Bogard, DD Garrison, DH TI Graves Nunataks 95209: A snapshot of metal segregation and core formation SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID INTERPLANETARY DUST PARTICLES; TRANSMISSION ELECTRON-MICROSCOPE; GRANULITE-FACIES GRAPHITE; ORDINARY CHONDRITES; ACAPULCO METEORITE; PARENT BODY; ISOTOPIC COMPOSITION; NITROGEN ISOTOPE; THERMAL HISTORY; OXYGEN-ISOTOPE AB GRA 95209 may provide our best opportunity to date to understand the earliest stages of core formation in asteroidal bodies. This lodranite preserves a physically, chemically, and mineralogically complex set of metal-sulfide veins. High-resolution X-ray computed tomography revealed three distinct lithologies. The dominant mixed metal-silicate-sulfide matrix is cut by metal-rich, graphite-bearing veins exceeding I cm in width and grades into a volumetrically minor metal-poor region. Silicate compositions and modal abundances are typical for lodranites, while the mineralogy of the metal-sulfide component is complex and differs among the three lithologies. Kamacite and troilite occur with chromite, tetrataenite, schreibersite, graphite, and a range of phosphates. An Ar-39-Ar-40 age of 4.521 +/- 0.006 Ga measures the time of closure of the K-Ar system. Carbon rosettes within the metal-rich vein are nitrogen-poor, well crystallized, include kamacite sub-grains of composition comparable to the host metal, and are essentially isotopically homogeneous (delta(13)C similar to -33 parts per thousand). In contrast, carbon rosettes within metal of the metal-poor lithology are N-poor, poorly crystallized, include kamacite grains that are Ni-poor compared to their host metal, and are isotopically heterogeneous (delta(13)C ranging from -50 to +80 parts per thousand) even within a single metal grain. The silicate portion of GRA 95209 is similar to the lodranite EET 84302, sharing a common texture, silicate mineral compositions, and Ar-Ar age. GRA 95209 and EET 84302 are intermediate between acapulcoites and lodranites. Both experienced Fe,Ni-FeS melting with extensive melt migration, but record only the onset of silicate partial melting with limited migration of silicate melt. The complex metal-sulfide veins in GRA 95209 resulted from low-degree partial melting and melt migration and intruded the matrix lithology. Reactions between solid minerals and melt, including oxidation-reduction reactions, produced the array of phosphates, schreibersite, and tetrataenite. Extensive reduction in the metal-rich vein resulted from its origin in a hotter portion of the asteroid. This difference in thermal history is supported by the graphite structures and isotopic compositions. The graphite rosettes in the metal-rich vein are consistent with high-temperature igneous processing. In contrast, the carbon in the metal-poor lithology appears to preserve a record of formation in the nebula prior to parent-body formation. Carbon incorporated from the solar nebula into a differentiating asteroid is preferentially incorporated in metal-sulfide melts that form a core, but does not achieve isotopic homogeneity until extensive thermal processing occurs. (c) 2005 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Lyndon B Johnson Space Ctr, AREA, Code KA, Houston, TX 77058 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM mccoy.tim@nmnh.si.edu RI Carlson, William/A-5807-2008; Stroud, Rhonda/C-5503-2008 OI Carlson, William/0000-0002-2954-5886; Stroud, Rhonda/0000-0001-5242-8015 NR 56 TC 26 Z9 26 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JAN 15 PY 2006 VL 70 IS 2 BP 516 EP 531 DI 10.1016/j.gca.2005.09.019 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 009PI UT WOS:000235124000016 ER PT J AU Luhr, JF Haldar, D AF Luhr, JF Haldar, D TI Barren Island Volcano (NE Indian Ocean): Island-arc high-alumina basalts produced by troctolite contamination SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Review DE active volcano; high-alumina basalt; island-arc; assimilation; anorthite ID HIGH-AN PLAGIOCLASE; EJECTED PLUTONIC BLOCKS; MID-ATLANTIC RIDGE; EAST PACIFIC RISE; SUBDUCTION ZONE; MELT INCLUSIONS; PHASE-RELATIONS; CARBON-DIOXIDE; TEMPORAL VARIATION; SOUFRIERE VOLCANO AB Barren Island (BI) is a subduction-related volcanic island lying in the northeastern Indian Ocean, about 750 km north of the northern tip of Sumatra. Rising from a depth of similar to 2300 in oil the Andaman Sea floor, BI has a submarine volume estimated at similar to 400 km(3), but the island is just 3 km across, reaches a maximum elevation of 355 m, and has a subaerial volume of only similar to 1.3 km(3). The first historical eruption began in 1787 when a cinder cone grew in the center of a pre-historical caldera 2-km in diameter and sent lava flows westward to reach the sea; activity continued intermittently until 1832. Two subsequent eruptions modified the central cone and also sent lava flows westward to reach the sea in 1991 and 1994-1995. A suite of 28 lava, scoria, and ash samples were investigated from various stages of the subaerial eruptive history of BI. Most are basalts (including all 10 samples from the 1994-1995 eruption) and basaltic andesites (including 7 of 8 samples from the 1991 eruption), but 2 pre-1787 andesites were also studied. On multi-element spider diagrams the BI suite shows subparallel trends for most elements that reflect an important role for fractional crystallization, along with the characteristic depletions of Nb-Ta and enrichments of K-Rb-Pb found in other subduction-related island-arc suites. The typical relative enrichment of Ba is not present, likely because the subducted sediments in the Andaman arc are not Ba-rich. Wide compositional ranges for Cs, Th, Rb, U, and Pb may trace different degrees of scavenging from the underlying volcanic pile. BI basalts and basaltic andesites have variable abundances of phenocrystic-microphenocrystic olivine plus Cr-Al-Mg spine] inclusions, plagioclase, and clinopyroxene, embedded in a matrix of glass, the same minerals, and titanomagnetite (mostly exsolved). The most remarkable mineralogical feature of certain BI basalts and basaltic andesites is the presence of abundant (to 40 vol.%) and large (to 5 mm) crystals of relatively homogeneous anorthitic plagioclase (to An(95.7)). These have inclusions of Mg olivine (to Fo(79)) and thin (10-150 mu m) normally zoned margins that reach to the more sodic compositions of the plagioclase phenocryst and microphenocryst rims. Anorthitic plagioclase crystals are common at many subduction-related volcanoes. At BI, the anorthitic plagioclase and associated olivine crystals are thought to have entered the magmas through disaggregation of troctolitic crystal mushes or plutonic xenoliths. This process affected bulk-rock compositions in many ways, including raising Al2O3 contents to values as high as 22.8 wt.% and Eu/Eu* values up to 1.05. Compared to a large petrological and geochemical database for Indonesian volcanic rocks, the BI suite falls at the most depleted end for levels of K and incompatible trace elements, and Sr, Nd, and Pb isotopic ratios. Consequently, the BI suite defines an excellent primitive baseline against which Indonesian volcanic suites can be compared. Published by Elsevier B.V. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. Presidency Coll, Dept Geol, Kolkata 700073, W Bengal, India. RP Luhr, JF (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,NHB 119, Washington, DC 20013 USA. EM luhr@volcano.si.edu; haldar2115@yahoo.co.uk NR 124 TC 71 Z9 79 U1 3 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 EI 1872-6097 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JAN 15 PY 2006 VL 149 IS 3-4 BP 177 EP 212 DI 10.1016/j.jvolgeores.2005.06.003 PG 36 WC Geosciences, Multidisciplinary SC Geology GA 005PO UT WOS:000234836500001 ER PT J AU Golombek, MP Crumpler, LS Grant, JA Greeley, R Cabrol, NA Parker, TJ Rice, JW Ward, JG Arvidson, RE Moersch, JE Fergason, RL Christensen, PR Castano, A Castano, R Haldemann, AFC Li, R Bell, JF Squyres, SW AF Golombek, MP Crumpler, LS Grant, JA Greeley, R Cabrol, NA Parker, TJ Rice, JW Ward, JG Arvidson, RE Moersch, JE Fergason, RL Christensen, PR Castano, A Castano, R Haldemann, AFC Li, R Bell, JF Squyres, SW TI Geology of the Gusev cratered plains from the Spirit rover transverse SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SIZE-FREQUENCY DISTRIBUTIONS; LANDING SITE PREDICTIONS; MINI-TES EXPERIMENT; MAADIM-VALLIS; MARS PATHFINDER; BRITTLE SOLIDS; FRAGMENT SIZE; ROCKS; RATES; SURFACE AB [1] The cratered plains of Gusev traversed by Spirit are generally low-relief rocky plains dominated by impact and eolian processes. Ubiquitous shallow, soil-filled, circular depressions, called hollows, are modified impact craters. Rocks are dark, fine-grained basalts, and the upper 10 m of the cratered plains appears to be an impact-generated regolith developed over intact basalt flows. Systematic field observations across the cratered plains identified vesicular clasts and rare scoria similar to original lava flow tops, consistent with an upper inflated surface of lava flows with adjacent collapse depressions. Crater and hollow morphometry are consistent with most being secondaries. The size-frequency distribution of rocks > 0.1 m diameter generally follows exponential functions similar to other landing sites for total rock abundances of 5-35%. Systematic clast counts show that areas with higher rock abundance and more large rocks have higher thermal inertia. Plains with lower thermal inertia have fewer rocks and substantially more pebbles that are well sorted and evenly spaced, similar to a desert pavement or lag. Eolian bed forms (ripples and wind tails) have coarse surface lags, and many are dust covered and thus likely inactive. Deflation of the surface similar to 5-25 cm likely exposed two-toned rocks and elevated ventifacts and transported fines into craters creating the hollows. This observed redistribution yields extremely slow average erosion rates of similar to 0.03 nm/yr and argues for very little long-term net change of the surface and a dry and desiccating environment similar to today's since the Hesperian (or similar to 3 Ga). C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM USA. Smithsonian Inst, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM mgolombek@jpl.nasa.gov RI Moersch, Jeffrey/F-7189-2010 NR 79 TC 63 Z9 64 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 12 PY 2006 VL 111 IS E2 AR E02S07 DI 10.1029/2005JE002503 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 007UT UT WOS:000234996400002 ER PT J AU Li, RX Archinal, BA Arvidson, RE Bell, J Christensen, P Crumpler, L Des Marais, DJ Di, KC Duxbury, T Golombek, M Grant, J Greeley, R Guinn, J Johnson, A Kirk, RL Maimone, M Matthies, LH Malin, M Parker, T Sims, M Thompson, S Squyres, SW Soderblom, LA AF Li, RX Archinal, BA Arvidson, RE Bell, J Christensen, P Crumpler, L Des Marais, DJ Di, KC Duxbury, T Golombek, M Grant, J Greeley, R Guinn, J Johnson, A Kirk, RL Maimone, M Matthies, LH Malin, M Parker, T Sims, M Thompson, S Squyres, SW Soderblom, LA TI Spirit rover localization and topographic mapping at the landing site of Gusev crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article AB [1] By sol 440, the Spirit rover has traversed a distance of 3.76 km (actual distance traveled instead of odometry). Localization of the lander and the rover along the traverse has been successfully performed at the Gusev crater landing site. We localized the lander in the Gusev crater using two-way Doppler radio positioning and cartographic triangulations through landmarks visible in both orbital and ground images. Additional high-resolution orbital images were used to verify the determined lander position. Visual odometry and bundle adjustment technologies were applied to compensate for wheel slippage, azimuthal angle drift, and other navigation errors (which were as large as 10.5% in the Husband Hill area). We generated topographic products, including 72 ortho maps and three-dimensional (3-D) digital terrain models, 11 horizontal and vertical traverse profiles, and one 3-D crater model (up to sol 440). Also discussed in this paper are uses of the data for science operations planning, geological traverse surveys, surveys of wind-related features, and other science applications. C1 Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. Smithsonian Inst, Washington, DC 20560 USA. Malin Space Sci Syst, San Diego, CA 92191 USA. RP Li, RX (reprint author), Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. EM li.282@osu.edu NR 28 TC 26 Z9 27 U1 2 U2 2 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 JAN 12 PY 2006 VL 111 IS E2 AR E02S06 DI 10.1029/2005JE002486 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 007UT UT WOS:000234996400001 ER PT J AU Petit, JM Holman, MJ Gladman, BJ Kavelaars, JJ Scholl, H Loredo, TJ AF Petit, JM Holman, MJ Gladman, BJ Kavelaars, JJ Scholl, H Loredo, TJ TI The Kuiper Belt luminosity function from m(R) =22 to 25 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; astrometry; Kuiper Belt; Solar system : formation ID TRANS-NEPTUNIAN OBJECTS; SIZE DISTRIBUTION; CENTAURS; BODIES; LIMITS; PLANE AB In summer 1999, we performed a survey optimized for the discovery of irregular satellites of Uranus and Neptune. We imaged 11.85 deg(2) of sky and discovered 66 new outer Solar system objects (not counting the three new Uranian satellites). Given the very short orbital arcs of our observations, only the heliocentric distance can be reliably determined. We were able to model the radial distribution of trans-Neptunian objects (TNOs). Our data support the idea of a strong depletion in the surface density beyond 45 au. After fully characterizing this survey's detection efficiency as a function of object magnitude and rate of motion, we find that the apparent luminosity function of the trans-Neptunian region in the range m(R) = 22 - 25 is steep with a best-fitting cumulative power-law index of alpha similar or equal to 0.76 with one object per deg(2) estimated at magnitude R-o = 23.3. This steep slope, corresponding to a differential size index of q similar or equal to 4.8, agrees with other older and more recent analyses for the luminosity function brighter than 25 mag. A double power-law fit to the new data set turns out to be statistically unwarrented; this large and homogeneous data set provides no evidence for a break in the power-law slope, which must eventually occur if the Bernstein et al. sky density measurements are correct. C1 Observ Besancon, F-25010 Besancon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Cote Azur, F-06304 Nice, France. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Petit, JM (reprint author), Observ Besancon, BP 1615, F-25010 Besancon, France. EM petit@obs-besancon.fr NR 27 TC 42 Z9 42 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 JAN 11 PY 2006 VL 365 IS 2 BP 429 EP 438 DI 10.1111/j.1365-2966.2005.09661.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VU UT WOS:000234853500006 ER PT J AU Maughan, BJ Jones, LR Ebeling, H Scharf, C AF Maughan, BJ Jones, LR Ebeling, H Scharf, C TI The evolution of the cluster X-ray scaling relations in the Wide Angle ROSAT Pointed Survey sample at 0.6 < z < 1.0 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : high-redshift; intergalactic medium; cosmology : observations; X-rays : galaxies ID XMM-NEWTON OBSERVATIONS; LUMINOSITY-TEMPERATURE RELATION; REDSHIFT GALAXY CLUSTERS; WARPS SURVEY; T RELATION; PROJECT; CHANDRA; GAS; ENTROPY; CONSTRAINTS AB The X-ray properties of a sample of 11 high-redshift (0.6 < z < 1.0) clusters observed with Chandra and/or XMM - Newton are used to investigate the evolution of the cluster scaling relations. The observed evolution in the normalization of the L - T, M - T, M-g - T and M - L relations is consistent with simple self-similar predictions, in which the properties of clusters reflect the properties of the Universe at their redshift of observation. Under the assumption that the model of self-similar evolution is correct and that the local systems formed via a single spherical collapse, the high-redshift L - T relation is consistent with the high-z clusters having virialized at a significantly higher redshift than the local systems. The data are also consistent with the more realistic scenario of clusters forming via the continuous accretion of material. The slope of the L - T relation at high redshift ( B = 3.32 +/- 0.37) is consistent with the local relation, and significantly steeper than the self-similar prediction of B = 2. This suggests that the same non-gravitational processes are responsible for steepening the local and high-z relations, possibly occurring universally at z greater than or similar to 1 or in the early stages of the cluster formation, prior to their observation. The properties of the intracluster medium at high redshift are found to be similar to those in the local Universe. The mean surface-brightness profile slope for the sample is beta = 0.66 +/- 0.05, the mean gas mass fractions within R-2500(z) and R-200(z) are 0.069 +/- 0.012 and 0.11 +/- 0.02, respectively, and the mean metallicity of the sample is 0.28 +/- 0.11 Z(.). C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM bmaughan@cfa.harvard.edu NR 43 TC 80 Z9 80 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 11 PY 2006 VL 365 IS 2 BP 509 EP 529 DI 10.1111/j.1365-2966.2005.09717.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VU UT WOS:000234853500014 ER PT J AU Rice, MS Martini, P Greene, JE Pogge, RW Shields, JC Mulchaey, JS Regan, MW AF Rice, MS Martini, P Greene, JE Pogge, RW Shields, JC Mulchaey, JS Regan, MW TI Spatially resolved narrow-line region kinematics in active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : Seyfert ID BLACK-HOLE MASS; JET-INDUCED VELOCITIES; SEYFERT-GALAXIES; GASEOUS KINEMATICS; CIRCUMNUCLEAR ENVIRONMENT; VIRIAL PARAMETER; EMISSION; PROFILES; STELLAR; DISPERSION AB We have analyzed Hubble Space Telescope spectroscopy of 24 nearby active galactic nuclei (AGNs) to investigate spatially resolved gas kinematics in the narrow-line region ( NLR). These observations effectively isolate the nuclear line profiles on less than 100 pc scales and are used to investigate the origin of the substantial scatter between the widths of strong NLR lines and the stellar velocity dispersion sigma* of the host galaxy, a quantity that relates with substantially less scatter to the mass of the central, supermassive black hole and more generally characterize variations in the NLR velocity field with radius. We find that line widths measured with STIS at a range of spatial scales systematically underestimate both sigma(*) and the line width measured from ground- based observations, although they do have comparably large scatter to the relation between ground- based NLR line width and sigma(*). There are no obvious trends in the residuals when compared with a range of host galaxy and nuclear properties. The widths and asymmetries of [O III] lambda 5007 and [S II] lambda lambda 6716, 6731 as a function of radius exhibit a wide range of behavior. Some of the most common phenomena are substantial width increases from the STIS to the large- scale, ground- based aperture and almost no change in line profile between the unresolved nuclear spectrum and ground-based measurements. We identify asymmetries in a surprisingly large fraction of low-ionization [S II] line profiles and several examples of substantial red asymmetries in both [O III] and [S II]. These results underscore the complexity of the circumnuclear material that constitutes the NLR and suggest that the scatter in the NLR width and sigma(*) correlation cannot be substantially reduced with a simple set of empirical relations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Rice, MS (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. EM martini@astronomy.ohio-state.edu NR 48 TC 21 Z9 21 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 JAN 10 PY 2006 VL 636 IS 2 BP 654 EP 673 DI 10.1086/498091 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400007 ER PT J AU Sakamoto, K Ho, PTP Iono, D Keto, ER Mao, RQ Matsushita, S Peck, AB Wiedner, MC Wilner, DJ Zhao, JH AF Sakamoto, K Ho, PTP Iono, D Keto, ER Mao, RQ Matsushita, S Peck, AB Wiedner, MC Wilner, DJ Zhao, JH TI Molecular superbubbles in the starburst galaxy NGC 253 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual ( NGC 253); galaxies : ISM; galaxies : starburst; ISM : bubbles ID SUPER-STAR CLUSTER; NGC 253; INTERSTELLAR-MEDIUM; NEARBY GALAXIES; DENSE GAS; CHANDRA OBSERVATIONS; NUCLEAR STARBURST; MICRON EMISSION; SPIRAL GALAXIES; M82 AB The central 2; 1 kpc of the starburst galaxy NGC 253 have been imaged using the Submillimeter Array at a 60 pc resolution in the J = 2 - 1 transitions of (12)CO, (13)CO, and C(18)O, as well as in the 1.3 mm continuum. Molecular gas and dust are distributed mainly in a circumnuclear disk of similar to 500 pc radius, with warm (similar to 40 K) and high area filling factor gas in its central part. Two gas shells or cavities have been discovered in the circumnuclear disk. They have similar to 100 pc diameters and have large velocity widths of 80 - 100 km s(-1), suggestive of expansion at similar to 50 km s(-1) . Modeled as an expanding bubble, each shell has an age of similar to 0.5 Myr and needed kinetic energy of similar to 1; 10(46) J, as well as mean mechanical luminosity of similar to 1; 10(33) W, for its formation. The large energy allows each to be called a superbubble. A similar to 10(6) M circle dot super star cluster can provide the luminosity and could be a building block of the nuclear starburst in NGC 253. Alternatively, a hypernova can also be the main source of energy for each superbubble, not only because it can provide the mechanical energy and luminosity but also because the estimated rate of superbubble formation and that of hypernova explosions are comparable. Our observations indicate that the circumnuclear molecular disk harboring the starburst is highly disturbed on 100 pc or smaller scales, presumably by individual young clusters and stellar explosions, in addition to being globally disturbed in the form of the well-known superwind. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96720 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Sakamoto, K (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array, 645 N Aohoku Pl, Hilo, HI 96720 USA. NR 86 TC 42 Z9 42 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 JAN 10 PY 2006 VL 636 IS 2 BP 685 EP 697 DI 10.1086/498075 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400010 ER PT J AU Rosenberg, JL Ashby, MLN Salzer, JJ Huang, JS Huang, S AF Rosenberg, JL Ashby, MLN Salzer, JJ Huang, JS Huang, S TI The diverse infrared properties of a complete sample of star-forming dwarf galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : abundances; galaxies : dwarf; galaxies : starburst; infrared : galaxies ID INTERNATIONAL SPECTROSCOPIC SURVEY; EMISSION-LINE GALAXIES; METALLICITY-LUMINOSITY RELATION; SPITZER-SPACE-TELESCOPE; ARRAY CAMERA IRAC; SURVEY LIST; METAL ABUNDANCES; KISS GALAXIES; OXYGEN ABUNDANCES; SBS 0335-052 AB We present mid-infrared Spitzer Space Telescope observations of a complete sample of star-forming dwarf galaxies selected from the KPNO International Spectroscopic Survey. The galaxies span a wide range in mid-infrared properties. Contrary to expectations, some of the galaxies emit strongly at 8 mu m, indicating the presence of hot dust and/or PAHs. The ratio of this mid-infrared dust emission to the stellar emission is compared with the galaxies' luminosity, star formation rate, metallicity, and optical reddening. We find that the ratio of the 8.0 mu m dust emission to the stellar emission is more strongly correlated with the star formation rate than it is with the metallicity or the optical reddening in these systems. Nonetheless, there is a correlation between the 8.0 mu m luminosity and metallicity. The slope of this luminosity-metallicity correlation is shallower than corresponding ones in the B band and 3.6 mu m. The precise nature of the 8.0 mu m emission seen in these galaxies (i. e., PAH vs. hot dust or some combination of the two) will require future study, including deep mid-IR spectroscopy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 65, Cambridge, MA 02138 USA. EM jlrosenberg@cfa.harvard.edu NR 46 TC 57 Z9 57 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2006 VL 636 IS 2 BP 742 EP 752 DI 10.1086/498133 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400014 ER PT J AU Fesen, RA Hammell, MC Morse, J Chevalier, RA Borkowski, KJ Dopita, MA Gerardy, CL Lawrence, SS Raymond, JC van den Bergh, S AF Fesen, RA Hammell, MC Morse, J Chevalier, RA Borkowski, KJ Dopita, MA Gerardy, CL Lawrence, SS Raymond, JC van den Bergh, S TI Discovery of outlying high-velocity oxygen-rich ejecta in Cassiopeia A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (Cassiopeia A); ISM : kinematics and dynamics; supernova remnants ID HUBBLE-SPACE-TELESCOPE; SUPER-NOVA REMNANT; X-RAY; PRESUPERNOVA EVOLUTION; PHYSICAL CONDITIONS; ADVANCED CAMERA; PROPER MOTIONS; MASSIVE STARS; EXPLOSION; SPECTRA AB Analysis of broadband HST ACS and WFPC2 images of the young Galactic supernova remnant Cassiopeia A reveals a far larger population of outlying, high-velocity knots of ejecta with a broader range of chemical properties than previously suspected. In this paper, we concentrate on a similar or equal to 1.5 arcmin(2) region located along the eastern limb of the remnant where we identify three main classes of outer ejecta: (1) knots dominated by [N(II)] lambda lambda 6548, 6583 emission, (2) knots dominated by oxygen emission lines, especially [O(II)] lambda lambda 7319, 7330, and (3) knots with emission-line strengths similar to the [S(II)]-strong fast-moving knot (FMK) ejecta commonly seen in the main emission shell. Mean transverse velocities derived from observed proper motion for N-rich, O-rich, and FMK-like knots identified in this region were found to be 8100, 7900, and 7600 km s(-1), respectively. The discovery of a significant population of O-rich ejecta situated between the suspected N-rich outer photospheric layer and S-rich FMK-like ejecta suggests that the progenitor's chemical layers were not completely disrupted by the supernova explosion outside of the remnant's northeast and southwest high-velocity "jet'' regions. In addition, we find the majority of O-rich outer ejecta at projected locations out beyond the remnant's fastest moving Fe-rich X-ray emission material seen in Chandra and XMM-Newton data along the eastern limb, suggesting that penetration of Fe-rich material up through the S-and Si-rich mantle did not extend past the progenitor's N- or O-rich outer layers for this section of the remnant. C1 Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Dominion Astrophys Observ, Herzberg Inst Astrophys, NRC Canada, Victoria, BC V9E 2E7, Canada. RP Fesen, RA (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 NR 48 TC 39 Z9 39 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 JAN 10 PY 2006 VL 636 IS 2 BP 859 EP 872 DI 10.1086/498092 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400023 ER PT J AU Seward, FD Gorenstein, P Smith, RK AF Seward, FD Gorenstein, P Smith, RK TI Chandra observations of the X-ray halo around the Crab Nebula SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Crab Nebula); supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; INTERSTELLAR GRAINS; SUPERNOVA-REMNANTS; SYNCHROTRON NEBULA; DUST; SCATTERING; PULSAR; EMISSION; SHELL; CONSTRAINTS AB Two Chandra observations have been used to search for thermal X-ray emission from within and around the Crab Nebula. Dead time was minimized by excluding the brightest part of the nebula from the field of view. A dust-scattered halo comprising 5% of the strength of the Crab is clearly detected, with surface brightness measured out to a radial distance of 18'. Coverage is 100% at 4', 50% at 12', and 25% at 18'. The observed halo is compared with predictions based on three different interstellar grain models, and one can be adjusted to fit the observation. This dust halo and mirror scattering form a high background region that has been searched for emission from shock-heated material in an outer shell. We find no evidence for such emission. We can set upper limits a factor of 10 - 1000 less than the surface brightness observed from outer shells around similar remnants. The upper limit for X-ray luminosity of an outer shell is approximate to 10(34) ergs s(-1). Although it is possible to reconcile our observation with an 8 - 13 M circle dot progenitor, we argue that this is unlikely. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Seward, FD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 22 Z9 22 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 JAN 10 PY 2006 VL 636 IS 2 BP 873 EP 880 DI 10.1086/498105 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400024 ER PT J AU Williams, JP Lee, CW Myers, PC AF Williams, JP Lee, CW Myers, PC TI High-resolution comparative study of the slowly contracting starless cores L694-2 and L1544 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L694, L1544); ISM : kinematics and dynamics; stars : formation ID MONTE-CARLO METHOD; PROTOSTELLAR COLLAPSE; INFALL MOTIONS; INTERSTELLAR CLOUDS; RADIATIVE-TRANSFER; LINE-PROFILES; DARK CLOUDS; CS 2-1; N2H+; MODELS AB We present interferometric observations of N(2)H(+)(1-0) in the starless, dense core L694-2 and compare them to previously published maps of L1544. Both cores are starless, centrally condensed, and show spectral signatures of rotation and collapse. We fit radially averaged spectra using a two-layer infall model and measure the variation of opacity and infall speed in each core. Both functions increase toward the center of each core, but the radial gradients are shallower, and the central values lower, in L694-2. This general behavior is predicted in models of gravitational collapse with thermal plus magnetic support, and the lower values in L694-2 may be due to its lower mass or a slightly earlier evolutionary state. In either case, it appears that both cores will form stars within a few 10(4) yr. C1 Inst Astron, Honolulu, HI 96822 USA. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Williams, JP (reprint author), Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jpw@ifa.hawaii.edu; cwl@kasi.re.kr; pmyers@cfa.harvard.edu RI Williams, Jonathan/B-1643-2009; OI Williams, Jonathan/0000-0001-5058-695X NR 44 TC 22 Z9 22 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 JAN 10 PY 2006 VL 636 IS 2 BP 952 EP 958 DI 10.1086/498231 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400032 ER PT J AU Sokoloski, JL Kenyon, SJ Espey, BR Keyes, CD McCandliss, SR Kong, AKH Aufdenberg, JP Filippenko, AV Li, W Brocksopp, C Kaiser, CR Charles, PA Rupen, MP Stone, RPS AF Sokoloski, JL Kenyon, SJ Espey, BR Keyes, CD McCandliss, SR Kong, AKH Aufdenberg, JP Filippenko, AV Li, W Brocksopp, C Kaiser, CR Charles, PA Rupen, MP Stone, RPS TI A "combination nova" outburst in Z andromedae: Nuclear shell burning triggered by a disk instability SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; novae, cataclysmic variables; stars : dwarf novae; stars : individual ( Z Andromedae); stars : winds, outflows; X-rays : binaries ID ACCRETING WHITE-DWARFS; SYMBIOTIC BINARY-Z; X-RAY SOURCES; IN-ORBIT PERFORMANCE; STAR Z-ANDROMEDAE; HOT COMPONENT; LOW-MASS; EG-AND; ULTRAVIOLET; LUMINOSITY AB We describe observational evidence for a new kind of interacting binary star outburst that involves both an accretion instability and an increase in thermonuclear shell burning on the surface of an accreting white dwarf. We refer to this new type of eruption as a combination nova. In late 2000, the prototypical symbiotic star Z Andromedae brightened by roughly 2mag in the optical. We observed the outburst in the radio with the VLA and MERLIN, in the optical both photometrically and spectroscopically, in the far-ultraviolet with FUSE, and in the X-rays with both Chandra and XMM-Newton. The 2 year long event had three distinct stages. During the first stage, the optical rise closely resembled an earlier, small outburst that was caused by an accretion disk instability. In the second stage, the hot component ejected an optically thick shell of material. In the third stage, the shell cleared to reveal a white dwarf whose luminosity remained on the order of 10(4) L(circle dot) for approximately 1 yr. The eruption was thus too energetic to have been powered by accretion alone. We propose that the initial burst of accretion was large enough to trigger enhanced nuclear burning on the surface of the white dwarf and the ejection of an optically thick shell of material. This outburst therefore combined elements of both a dwarf nova and a classical nova. Our results have implications for the long-standing problem of producing shell flashes with short recurrence times on low-mass white dwarfs in symbiotic stars. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Univ Calif Berkeley, Astron Dept, Berkeley, CA 94720 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Southampton, Southampton S017 1BJ, Hants, England. S African Astron Observ, ZA-7935 Observatory, South Africa. NRAO, Socorro, NM 87801 USA. UCO Lick Observ, Mt Hamilton, CA 95140 USA. RP Sokoloski, JL (reprint author), Smithsonian Astrophys Observ, 60 Gdn St, Cambridge, MA 02138 USA. EM jsokolos@cfa.harvard.edu OI Espey, Brian/0000-0002-2457-1380; Kenyon, Scott/0000-0003-0214-609X NR 83 TC 68 Z9 69 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 JAN 10 PY 2006 VL 636 IS 2 BP 1002 EP 1019 DI 10.1086/498206 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NR UT WOS:000234469400039 ER PT J AU Foster, JB Goodman, AA AF Foster, JB Goodman, AA TI Cloudshine: New light on dark clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : structure ID SURFACE BRIGHTNESS; INTERSTELLAR DUST; NEBULAE; SCATTERING; EMISSION; GRAINS AB We present new deep near-infrared images of dark clouds in the Perseus molecular complex. These images show beautiful extended emission that we model as scattered ambient starlight and name "cloudshine." The brightness and color variation of cloudshine complicates the production of extinction maps, the best tracer of column density in clouds. However, since the profile of reflected light is essentially a function of mass distribution, cloudshine provides a new way to study the structure of dark clouds. Previous work has used optical scattered light to study the density profile of tenuous clouds; extending this technique into the infrared provides a high-resolution view into the interiors of very dense clouds, bypassing the complexities of using thermal dust emission, which is biased by grain temperature, or molecular tracers, which have complicated depletion patterns. As new wide-field infrared cameras are used to study star-forming regions at greater depth, cloudshine will be widely observed and should be seen as a new high-resolution tool, rather than an inconvenience. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foster, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 13 TC 39 Z9 39 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 JAN 10 PY 2006 VL 636 IS 2 BP L105 EP L108 DI 10.1086/500131 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700012 ER PT J AU Hirano, N Liu, SY Shang, H Ho, PTP Huang, HC Kuan, YJ McCaughrean, MJ Zhang, QZ AF Hirano, N Liu, SY Shang, H Ho, PTP Huang, HC Kuan, YJ McCaughrean, MJ Zhang, QZ TI SiO J=5-4 in the HH 211 protostellar jet imaged with the Submillimeter Array SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (HH 211); ISM : jets and outflows; ISM : molecules; shock waves; stars : formation ID MOLECULAR OUTFLOWS; EMISSION; DRIVEN AB We have mapped the SiO J = 5 - 4 line at 217 GHz from the HH 211 molecular outflow with the Submillimeter Array ( SMA). The high-resolution map (1 ''.6 x 0 ''.9) shows that the SiO J = 5 - 4 emission comes from the central narrow jet along the outflow axis with a width of similar to 0 ''.8 (similar to 250 AU) FWHM. The SiO jet consists of a chain of knots separated by 3 '' - 4 '' (similar to 1000 AU), and most of the SiO knots have counterparts in shocked H-2 emission seen in a new, deep VLT near-infrared image of the outflow. A new, innermost pair of knots have been discovered at just +/- 2 '' from the central star. The line ratio between the SiO J = 5 - 4 data and the upper limits from the SiO J = 1 - 0 data of Chandler & Richer suggests that these knots have a temperature in excess of 300 - 500 K and a density of (0.5 - 1) x 10(7) cm(-3). The radial velocity measured for these knots is similar to 30 km s(-1), comparable to the maximum velocity seen in the entire jet. The high temperature, high density, and velocity structure observed in this pair of SiO knots suggest that they are closely related to the primary jet launched close to the protostar. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. RP Hirano, N (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hirano@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 NR 18 TC 51 Z9 51 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 JAN 10 PY 2006 VL 636 IS 2 BP L141 EP L144 DI 10.1086/500201 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700021 ER PT J AU Lahuis, F van Dishoeck, EF Boogert, ACA Pontoppidan, KM Blake, GA Dullemond, CP Evans, NJ Hogerheijde, MR Jorgensen, JK Kessler-Silacci, JE Knez, C AF Lahuis, F van Dishoeck, EF Boogert, ACA Pontoppidan, KM Blake, GA Dullemond, CP Evans, NJ Hogerheijde, MR Jorgensen, JK Kessler-Silacci, JE Knez, C TI Hot organic molecules toward a young low-mass star: A look at inner disk chemistry SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : ISM; ISM : individual (IRS 46); ISM : jets and outflows; ISM : molecules; planetary systems : protoplanetary disks; stars : formation ID HERBIG-AE STARS; T-TAURI STARS; PROTOSTELLAR ENVELOPES; PROTOPLANETARY DISKS; CHEMICAL EVOLUTION; STELLAR OBJECTS; OPHIUCHI CLOUD; CO EMISSION; SPECTROSCOPY; GAS AB Spitzer Space Telescope spectra of the low-mass young stellar object (YSO) IRS 46 (L-bol approximate to 0.6 L-circle dot) in Ophiuchus reveal strong vibration-rotation absorption bands of gaseous C2H2, HCN, and CO2. This is the only source out of a sample of similar to 100 YSOs that shows these features, and this is the first time that they are seen in the spectrum of a solar-mass YSO. Analysis of the Spitzer data combined with Keck L- and M- band spectra reveals excitation temperatures of greater than or similar to 350 K and abundances of 10(-6) to 10(-5) with respect to H 2, orders of magnitude higher than those found in cold clouds. In spite of this high abundance, the HCN line is barely detected with the J = 4 - 3 James Clerk Maxwell Telescope (JCMT), indicating a source diameter less than 13 AU. The (sub) millimeter continuum emission and the absence of scattered light in near-infrared images limit the mass and temperature of any remnant collapsing envelope to less than 0.01 M-circle dot and 100 K, respectively. This excludes a hot-core - type region as found in high-mass YSOs. The most plausible origin of this hot gas rich in organic molecules is in the inner (< 6 AU radius) region of the disk around IRS 46, either the disk itself or a disk wind. A nearly edge-on two-dimensional disk model fits the spectral energy distribution (SED) and gives a column of dense warm gas along the line of sight that is consistent with the absorption data. These data illustrate the unique potential of high-resolution infrared spectroscopy to probe the organic chemistry, gas temperatures, and gas kinematics in the planet-forming zones close to a young star. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. SRON, Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lahuis, F (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM f.lahuis@sron.rug.nl OI Dullemond, Cornelis/0000-0002-7078-5910 NR 36 TC 79 Z9 79 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 JAN 10 PY 2006 VL 636 IS 2 BP L145 EP L148 DI 10.1086/500084 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700022 ER PT J AU Palau, A Ho, PTP Zhang, Q Estalella, R Hirano, N Shang, H Lee, CF Bourke, TL Beuther, H Kuan, YJ AF Palau, A Ho, PTP Zhang, Q Estalella, R Hirano, N Shang, H Lee, CF Bourke, TL Beuther, H Kuan, YJ TI Submillimeter emission from the hot molecular jet HH 211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (HH 211); ISM : jets and outflows; stars : formation ID PROTOSTELLAR JET; OUTFLOWS; SIO AB We observed the HH 211 jet in the submillimeter continuum and the CO ( 3 - 2) and SiO ( 8 - 7) transitions with the Submillimeter Array. The continuum source detected at the center of the outflow shows an elongated morphology, perpendicular to the direction of the outflow axis. The high- velocity emission of both molecules shows a knotty and highly collimated structure. The SiO ( 8 - 7) emission at the base of the outflow, close to the driving source, spans a wide range of velocities, from - 20 up to 40 km s (- 1). This suggests that a wide- angle wind may be the driving mechanism of the HH 211 outflow. For distances >= 5 (n) (similar to 1500 AU) from the driving source, emission from both transitions follows a Hubble- law behavior, with SiO ( 8 - 7) reaching higher velocities than CO ( 3 - 2) and being located upstream of the CO ( 3 - 2) knots. This indicates that the SiO ( 8 - 7) emission is likely tracing entrained gas very close to the primary jet, while the CO ( 3 - 2) is tracing less dense entrained gas. From the SiO ( 5 - 4) data of Hirano et al., we find that the SiO ( 8 - 7)/ SiO ( 5 - 4) brightness temperature ratio along the jet decreases for knots far from the driving source. This is consistent with the density decreasing along the jet, from cm (- 3) at 500 AU to cm (- 3) at 5000 AU from the driving source. C1 Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. RP Palau, A (reprint author), Univ Barcelona, Dept Astron & Meteorol, Av Diagonal 647, E-08028 Barcelona, Spain. OI Zhang, Qizhou/0000-0003-2384-6589 NR 15 TC 43 Z9 43 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 JAN 10 PY 2006 VL 636 IS 2 BP L137 EP L140 DI 10.1086/500242 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700020 ER PT J AU Qi, CH Wilner, DJ Calvet, N Bourke, TL Blake, GA Hogerheijde, MR Ho, PTP Bergin, E AF Qi, CH Wilner, DJ Calvet, N Bourke, TL Blake, GA Hogerheijde, MR Ho, PTP Bergin, E TI CO J=6-5 observations of TW Hydrae with the Submillimeter Array SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : molecules; planetary systems : protoplanetary disks; radio lines : stars; stars : individual (TW Hydrae) ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; X-RAY SPECTROSCOPY; PROTOPLANETARY DISK; CIRCUMSTELLAR DISKS; TAURI STARS; GAS; TEMPERATURE; ACCRETION; EMISSION AB We present the first images of the 691.473 GHz CO J = 6 - 5 line in a protoplanetary disk, obtained along with the 690 GHz dust continuum, toward the classical T Tauri star TW Hya, using the Submillimeter Array. Imaging in the CO J = 6 - 5 line reveals a rotating disk, consistent with previous observations of CO J = 3 - 2 and 2 - 1 lines. Using an irradiated accretion disk model and two-dimensional Monte Carlo radiative transfer, we find that additional surface heating is needed to simultaneously fit the absolute and relative intensities of the CO J = 6 - 5, 3 - 2, and 2 - 1 lines. In particular, the vertical gas temperature gradient in the disk must be steeper than that of the dust, mostly likely because the CO emission lines probe nearer to the surface of the disk. We have used an idealized X-ray heating model to fit the line profiles of CO J = 2 - 1 and 3 - 2 with chi(2) analysis, and the prediction of this model yields CO J = 6 - 5 emission consistent with the observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. EM cqi@cfa.harvard.edu; dwilner@cfa.harvard.edu; ncalvet@cfa.harvard.edu; tbourke@cfa.harvard.edu; gab@gps.caltech.edu; michiel@strw.leidenuniv.nl; ho@cfa.harvard.edu; ebergin@umich.edu NR 21 TC 68 Z9 68 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 JAN 10 PY 2006 VL 636 IS 2 BP L157 EP L160 DI 10.1086/500241 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700025 ER PT J AU Shafee, R McClintock, JE Narayan, R Davis, SW Li, LX Remillard, RA AF Shafee, R McClintock, JE Narayan, R Davis, SW Li, LX Remillard, RA TI Estimating the spin of stellar-mass black holes by spectral fitting of the X-ray continuum SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion,accretion disks; binaries : close; black hole physics; stars : individual (4U 1543-47, GRO J1655-40); X-rays : stars ID SOURCE GRO J1655-40; ORBITAL PARAMETERS; DISC MODEL; ACCRETION; OUTBURST; CANDIDATES; EVOLUTION; JETS AB We fit X-ray spectral data in the thermal-dominant, or high-soft, state of two dynamically confirmed black holes, GRO J1655-40 and 4U 1543-47, and estimate the dimensionless spin parameters a* a/M of the two holes. For GRO J1655-40, using a spectral hardening factor computed for a non-LTE relativistic accretion disk, we estimate a*similar to 0.75 and a*similar to 0.65-0.75, respectively, from ASCA and RXTE data. For 4U 1543-47, we estimate a*similar to 0.75-0.85 from RXTE data. Thus, neither black hole has a spin approaching the theoretical maximum a* = 1. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Shafee, R (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. NR 24 TC 189 Z9 189 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 JAN 10 PY 2006 VL 636 IS 2 BP L113 EP L116 DI 10.1086/498938 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000NU UT WOS:000234469700014 ER PT J AU Pickett, HM Drouin, BJ Canty, T Kovalenko, LJ Salawitch, RJ Livesey, NJ Read, WG Waters, JW Jucks, KW Traub, WA AF Pickett, HM Drouin, BJ Canty, T Kovalenko, LJ Salawitch, RJ Livesey, NJ Read, WG Waters, JW Jucks, KW Traub, WA TI Validation of Aura MLS HOx measurements with remote-sensing balloon instruments SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OH AB Satellite measurements of OH and HO2 obtained by the Aura MLS instrument are compared to the balloon-borne BOH and FIRS-2 instruments. All measurements are also compared with constrained photochemical model calculations. On average, both balloon measurements of OH agree with MLS within 17% over 25 - 40 km and the measurements agree with the model within 12%. The three measurements for column of OH above 40 km agree within 8% and the mean is 12% below the model. Measurements of HO2 from FIRS-2 and MLS agree on average within 23% over 25 - 40 km and the differences are generally within the experimental precision. The HO2 measurements agree with the model within 14%. Measurements of HO2 for the column over 40 - 60 km agree within 16% and the mean measured column agrees with the model within the experimental precision. Our observations do not appear to indicate a "HOx dilemma''. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pickett, HM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM herbert.m.pickett@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 8 TC 25 Z9 25 U1 0 U2 0 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 JAN 10 PY 2006 VL 33 IS 1 AR L01808 DI 10.1029/2005GL024048 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 007UE UT WOS:000234994700002 ER PT J AU Sumner, S Pereboom, JJM Jordan, WC AF Sumner, S Pereboom, JJM Jordan, WC TI Differential gene expression and phenotypic plasticity in behavioural castes of the primitively eusocial wasp, Polistes canadensis SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE paper wasp; social insect; caste determination; suppression subtractive hybridization ID SOCIAL WASP; JUVENILE-HORMONE; APIS-MELLIFERA; HONEY-BEE; HYMENOPTERA; ANNULARIS; EVOLUTION; GENOMICS; WORKERS; QUEENS AB Understanding how a single genome can produce a variety of different phenotypes is of fundamental importance in evolutionary and developmental biology. One of the most striking examples of phenotypic plasticity is the female caste system found in eusocial insects, where variation in reproductive (queens) and non-reproductive (workers) phenotypes results in a broad spectrum of caste types, ranging from behavioural through to morphological castes. Recent advances in genomic techniques allow novel comparisons on the nature of caste phenotypes to be made at the level of the genes in organisms for which there is little genome information, facilitating new approaches in studying social evolution and behaviour. Using the paper wasp Polistes canadensis as a model system, we investigated for the first time how behavioural castes in primitively eusocial insect societies are associated with differential expression of shared genes. We found that queens and newly emerged females express gene expression patterns that are distinct from each other whilst workers generally expressed intermediate patterns, as predicted by Polistes biology. We compared caste-associated genes in P canadensis with those expressed in adult queens and workers of more advanced eusocial societies, which represent four independent origins of eusociality. Nine genes were conserved across the four taxa, although their patterns of expression and putative functions varied. Thus, we identify several genes that are putatively of evolutionary importance in the molecular biology that underlies a number of caste systems of independent evolutionary origin. C1 Smithsonian Trop Res Inst, Balboa, Panama. Zool Soc London, Inst Zool, London NW1 4RY, England. Royal Zool Soc Antwerp, Ctr Res & Conservat, B-2018 Antwerp, Belgium. RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM seirian.sumner@ioz.ac.uk RI Sumner, Seirian/E-6611-2011 NR 42 TC 40 Z9 42 U1 8 U2 30 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 JAN 7 PY 2006 VL 273 IS 1582 BP 19 EP 26 DI 10.1098/rspb.2005.3291 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 002YL UT WOS:000234648100003 PM 16519229 ER PT J AU Arvidson, RE Squyres, SW Anderson, RC Bell, JF Blaney, D Bruckner, J Cabrol, NA Calvin, WM Carr, MH Christensen, PR Clark, BC Crumpler, L Des Marais, DJ de Souza, PA d'Uston, C Economou, T Farmer, J Farrand, WH Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Guinness, E Hahn, BC Haskin, L Herkenhoff, KE Hurowitz, JA Hviid, S Johnson, JR Klingelhofer, G Knoll, AH Landis, G Leff, C Lemmon, M Li, R Madsen, MB Malin, MC McLennan, SM McSween, HY Ming, DW Moersch, J Morris, RV Parker, T Rice, JW Richter, L Rieder, R Rodionov, DS Schroder, C Sims, M Smith, M Smith, P Soderblom, LA Sullivan, R Thompson, SD Tosca, NJ Wang, A Wanke, H Ward, J Wdowiak, T Wolff, M Yen, A AF Arvidson, RE Squyres, SW Anderson, RC Bell, JF Blaney, D Bruckner, J Cabrol, NA Calvin, WM Carr, MH Christensen, PR Clark, BC Crumpler, L Des Marais, DJ de Souza, PA d'Uston, C Economou, T Farmer, J Farrand, WH Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Guinness, E Hahn, BC Haskin, L Herkenhoff, KE Hurowitz, JA Hviid, S Johnson, JR Klingelhofer, G Knoll, AH Landis, G Leff, C Lemmon, M Li, R Madsen, MB Malin, MC McLennan, SM McSween, HY Ming, DW Moersch, J Morris, RV Parker, T Rice, JW Richter, L Rieder, R Rodionov, DS Schroder, C Sims, M Smith, M Smith, P Soderblom, LA Sullivan, R Thompson, SD Tosca, NJ Wang, A Wanke, H Ward, J Wdowiak, T Wolff, M Yen, A TI Overview of the Spirit Mars Exploration Rover Mission to Gusev Crater: Landing site to Backstay Rock in the Columbia Hills SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MINI-TES; SOILS; SPECTROMETER; OPPORTUNITY; MINERALOGY; CHEMISTRY AB Spirit landed on the floor of Gusev Crater and conducted initial operations on soil-covered, rock-strewn cratered plains underlain by olivine-bearing basalts. Plains surface rocks are covered by wind-blown dust and show evidence for surface enrichment of soluble species as vein and void-filling materials and coatings. The surface enrichment is the result of a minor amount of transport and deposition by aqueous processes. Layered granular deposits were discovered in the Columbia Hills, with outcrops that tend to dip conformably with the topography. The granular rocks are interpreted to be volcanic ash and/or impact ejecta deposits that have been modified by aqueous fluids during and/or after emplacement. Soils consist of basaltic deposits that are weakly cohesive, relatively poorly sorted, and covered by a veneer of wind-blown dust. The soils have been homogenized by wind transport over at least the several kilometer length scale traversed by the rover. Mobilization of soluble species has occurred within at least two soil deposits examined. The presence of monolayers of coarse sand on wind-blown bedforms, together with even spacing of granule-sized surface clasts, suggests that some of the soil surfaces encountered by Spirit have not been modified by wind for some time. On the other hand, dust deposits on the surface and rover deck have changed during the course of the mission. Detection of dust devils, monitoring of the dust opacity and lower boundary layer, and coordinated experiments with orbiters provided new insights into atmosphere-surface dynamics. C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Chem, D-55020 Mainz, Germany. NASA, Ames SETI Inst, Moffett Field, CA 94035 USA. Univ Nevada, Reno, NV 89557 USA. US Geol Survey, Menlo Pk, CA 94025 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Companhia Vale Rio Doce, BR-20030900 Rio De Janeiro, Brazil. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Space Sci Inst, Boulder, CO 80301 USA. Honeybee Robot, New York, NY 10012 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Massachusetts Inst Technol Earth Atmosphere & Pla, Cambridge, MA 02139 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Max Planck Inst Sonnensyst Forsch, Katlenburg Lindau, Germany. Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. Malin Space Sci Syst, San Diego, CA 92191 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. DLR Inst Space Simulat, Cologne, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA. Space Sci Inst, Martinez, GA USA. RP Washington Univ, Dept Earth & Planetary Sci, Campus Box 1169,1 Brookings Dr, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Moersch, Jeffrey/F-7189-2010; Lemmon, Mark/E-9983-2010; Johnson, Jeffrey/F-3972-2015; Madsen, Morten/D-2082-2011; Schroder, Christian/B-3870-2009; de Souza, Paulo/B-8961-2008; Smith, Michael/C-8875-2012; Hurowitz, Joel/A-8862-2008 OI Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111; Schroder, Christian/0000-0002-7935-6039; de Souza, Paulo/0000-0002-0091-8925; NR 43 TC 116 Z9 117 U1 3 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 6 PY 2006 VL 111 IS E2 AR E02S01 DI 10.1029/2005JE002499 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 001CG UT WOS:000234510100006 ER PT J AU Grant, JA Arvidson, RE Crumpler, LS Golombek, MP Hahn, B Haldemann, AFC Li, R Soderblom, LA Squyres, SW Wright, SP Watters, WA AF Grant, JA Arvidson, RE Crumpler, LS Golombek, MP Hahn, B Haldemann, AFC Li, R Soderblom, LA Squyres, SW Wright, SP Watters, WA TI Crater gradation in Gusev crater and Meridiani Planum, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ROVER LANDING SITE; IMPACT CRATERS; SPIRIT ROVER; EJECTA EMPLACEMENT; MICROSCOPIC IMAGER; TERRA-MERIDIANI; BURNS FORMATION; DEGRADATION; DEPOSITS; SOILS AB The Mars Exploration Rovers investigated numerous craters in Gusev crater and Meridiani Planum during the first similar to 400 sols of their missions. Craters vary in size and preservation state but are mostly due to secondary impacts at Gusev and primary impacts at Meridiani. Craters at both locations are modified primarily by eolian erosion and infilling and lack evidence for modification by aqueous processes. Effects of gradation on crater form are dependent on size, local lithology, slopes, and availability of mobile sediments. At Gusev, impacts into basaltic rubble create shallow craters and ejecta composed of resistant rocks. Ejecta initially experience eolian stripping, which becomes weathering-limited as lags develop on ejecta surfaces and sediments are trapped within craters. Subsequent eolian gradation depends on the slow production of fines by weathering and impacts and is accompanied by minor mass wasting. At Meridiani the sulfate-rich bedrock is more susceptible to eolian erosion, and exposed crater rims, walls, and ejecta are eroded, while lower interiors and low-relief surfaces are increasingly infilled and buried by mostly basaltic sediments. Eolian processes outpace early mass wasting, often produce meters of erosion, and mantle some surfaces. Some small craters were likely completely eroded/buried. Craters >100 m in diameter on the Hesperian-aged floor of Gusev are generally more pristine than on the Amazonian-aged Meridiani plains. This conclusion contradicts interpretations from orbital views, which do not readily distinguish crater gradation state at Meridiani and reveal apparently subdued crater forms at Gusev that may suggest more gradation than has occurred. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11790 USA. Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, 6th & Independence SW, Washington, DC 20560 USA. EM grantj@si.edu NR 50 TC 41 Z9 41 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JAN 6 PY 2006 VL 111 IS E2 AR E02S08 DI 10.1029/2005JE002465 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 001CG UT WOS:000234510100002 ER PT J AU Xu, Y Reid, MJ Zheng, XW Menten, KM AF Xu, Y Reid, MJ Zheng, XW Menten, KM TI The distance to the Perseus spiral arm in the Milky Way SO SCIENCE LA English DT Article ID GHZ METHANOL MASERS; KINEMATICS; GALAXIES; REGIONS; W3(OH) AB We have measured the distance to the massive star-forming region W3OH in the Perseus Spiral arm of the Milky Way to be 1.95 +/- 0.04 kitoparsecs (5.86 X 10(16) km). This distance was determined by triangulation, with Earth's orbit as one segment of a triangle, using the Very Long Baseline Array. This resolves the long-standing problem that there is a discrepancy of a factor of 2 between different techniques used to determine distances. The reason for the discrepancy is that this portion of the Perseus arm has anomalous motions. The orientation of the anomalous motion agrees with spiral density-wave theory, but the magnitude of the motion is somewhat larger than most models predict. C1 Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chinese Acad Sci, Shanghai Astron Observ, Shanghai, Peoples R China. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Xu, Y (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. NR 18 TC 188 Z9 196 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 JAN 6 PY 2006 VL 311 IS 5757 BP 54 EP 57 DI 10.1126/science.1120914 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 001ON UT WOS:000234546300029 PM 16339410 ER PT J AU Currie, CR Poulsen, M Mendenhall, J Boomsma, JJ Billen, J AF Currie, CR Poulsen, M Mendenhall, J Boomsma, JJ Billen, J TI Coevolved crypts and exocrine glands support mutualistic bacteria in fungus-growing ants SO SCIENCE LA English DT Article ID PHYLOGENETIC ANALYSIS; TRIPARTITE MUTUALISM; SYMBIOSIS; PARASITES; GARDENS AB Attine ants engage in a quadripartite symbiosis with fungi they cultivate for food, specialized garden parasites, and parasite-inhibiting bacteria. Molecular phylogenetic evidence supports an ancient host-pathogen association between the ant-cultivar mutualism and the garden parasite. Here we show that ants rear the antibiotic-producing bacteria in elaborate cuticular crypts, supported by unique exocrine glands, and that these structures have been highly modified across the ants' evolutionary history. This specialized structural evolution, together with the absence of these bacteria and modifications in other ant genera that do not grow fungus, indicate that the bacteria have an ancient and coevolved association with the ants, their fungal cultivar, and the garden parasite. C1 Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Copenhagen, Inst Biol, Dept Populat Biol, DK-2100 Copenhagen, Denmark. Univ Texas, Inst Mol & Cellular Biol, Austin, TX 78712 USA. Catholic Univ Louvain, Inst Zool, B-3000 Louvain, Belgium. RP Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM currie@bact.wisc.edu RI Boomsma, Jacobus/M-2785-2014; Poulsen, Michael/C-6276-2012; OI Boomsma, Jacobus/0000-0002-3598-1609; Poulsen, Michael/0000-0002-2839-1715; Billen, Johan/0000-0002-2392-7293 NR 20 TC 153 Z9 162 U1 5 U2 64 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JAN 6 PY 2006 VL 311 IS 5757 BP 81 EP 83 DI 10.1126/science.1119744 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 001ON UT WOS:000234546300037 PM 16400148 ER PT J AU Gould, A Dorsher, S Gaudi, BS Udalski, A AF Gould, A Dorsher, S Gaudi, BS Udalski, A TI Frequency of hot jupiters and very hot jupiters from the OGLE-III transit surveys toward the galactic bulge and carina SO ACTA ASTRONOMICA LA English DT Article DE planetary systems; binaries : eclipsing; Stars : fundamental parameters ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR GIANT PLANETS; DOPPLER FOLLOW-UP; SPECTRAL TYPES; 2001 CAMPAIGN; HOST STARS; CANDIDATES; SEARCH; DISK AB We derive the frequencies of hot Jupiters (HJs) with 3-5 day periods and very hot Jupiters (VHJs) with 1-3 day periods by comparing the planets actually detected in the OGLE-III survey with those predicted by our models. The models are constructed following Gould and Morgan (2003) by populating the line of sight with stars drawn from the Hipparcos Catalogue. Using these, we demonstrate that the number of stars with sensitivity to HJs and VHJs is only 5-16% of those in the OGLE-III fields satisfying the spectroscopic-follow-up limit of V-max, < 17.5 mag. Hence, the frequencies we derive are much higher than a naive estimate would indicate. We find that at 90% confidence the fraction of stars with planets in the two period ranges is (1 /320) ( (1+1.37)(-0.59)) for HJs and (1/710)((1+1.10)(-0.54)) for VHJs. The HJ rate is statistically indistinguishable from that found in radial velocity (RV) studies. However, we note that magnitude-limited RV samples are heavily biased toward metal-rich (hence, planet-bearing) stars, while transit surveys are not, and therefore we expect that more sensitive transit surveys should find a deficit of HJs as compared to RV surveys. The detection of three transiting VHJs, all with periods less than 2 days, is marginally consistent with the complete absence of such detections in RV surveys. The planets detected are consistent with being uniformly distributed between 1.00 and 1.25 Jovian radii, but there are too few in the sample to map this distribution in detail. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Warsaw Univ, Observ, PL-00478 Warsaw, Poland. RP Gould, A (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM gould@astronomy.ohio-state.edu; dorsher@astronomy.ohio-state.edu; sgaudi@cfa.harvard.edu; udalski@astrouw.edu.pl RI Gaudi, Bernard/I-7732-2012 NR 53 TC 53 Z9 53 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2006 VL 56 IS 1 BP 1 EP 50 PG 50 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 035PW UT WOS:000237014800001 ER PT J AU Pepper, J AF Pepper, J. TI Toward the detection of transiting hot earths and hot neptunes in open clusters SO ACTA ASTRONOMICA LA English DT Article DE open clusters and associations : general; techniques : photometric; surveys; planetary systems ID EXTRASOLAR PLANETS; STAR CLUSTER; STELLAR-SYSTEMS; GALACTIC BULGE; MASS PLANET; CFHT; RICH; AGE; PHOTOMETRY; TELESCOPE AB Radial velocity searches for extrasolar planets have recently detected several very low mass (7-20M(.)) planets in close orbits with periods <= 10 days. We consider the prospects for detecting the analogs of these planets in Galactic open clusters via transits. We outline the requirements for constructing a transit survey that would allow one to probe such "Hot Earths" and "Hot Neptunes." Specifically, we present a simple criterion for detection that defines the minimum aperture required to detect planets of a given radius in a cluster at a given distance. Adopting photometric precisions that have been demonstrated in state-of-the-art variability surveys, we then predict the number of planets one could potentially detect with ambitious transit surveys toward several open clusters. Dedicated surveys lasting more than 20 nights with Pan-STARRS toward the Hyades and Praesepe could detect a handful of Hot Earths, if the majority of stars host such planets. Similar surveys with larger aperture telescopes (e.g., CFHT, MMT), toward M 67, M 35, M 50, and M 37 could detect Hot Neptunes, provided that their frequency is >= 1%. The majority of planets will be detected around M dwarfs; detecting Hot Neptunes around such primaries requires photometric precisions of 1%, whereas Hot Earths require approximate to 0.1%. We discuss potential hurdles in detecting and confirming small planets in ground-based surveys, including correlated noise, false positives, and intrinsic stellar variability. C1 Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pepper, J (reprint author), Ohio State Univ, Dept Astron, McPherson Lab 4055, 140 W 18th Ave, Columbus, OH 43210 USA. EM pepper@astronomy.ohio-state.edu NR 43 TC 10 Z9 10 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2006 VL 56 IS 2 BP 183 EP 197 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 064RB UT WOS:000239105700003 ER PT J AU Stanek, KZ Gnedin, OY Beacom, JF Gould, AP Johnson, JA Kollmeier, JA Modjaz, M Pinsonneault, MH Pogge, R Weinberg, DH AF Stanek, K. Z. Gnedin, O. Y. Beacom, J. F. Gould, A. P. Johnson, J. A. Kollmeier, J. A. Modjaz, M. Pinsonneault, M. H. Pogge, R. Weinberg, D. H. TI Protecting life in the Milky Way: Metals keep the GRBs away SO ACTA ASTRONOMICA LA English DT Article DE gamma rays : bursts ID GAMMA-RAY BURSTS; STAR-FORMING GALAXIES; OXYGEN GALACTIC GRADIENTS; STELLAR MASS; LOW METALLICITY; HOST GALAXIES; CASSIOPEIA-A; LOW-REDSHIFT; SUPERNOVA; CONSTRAINTS AB The host galaxies of the five local, z <= 0.25, long-duration gamma-ray bursts (GRBs 980425, 020903, 030329, 031203 and 060218), each of which had a well-documented associated supernova, are all faint and metal-poor compared to the population of local star-forming galaxies. We quantify this statement by using a previous analysis of star-forming galaxies (0.005 < z < 0.2) from the Sloan Digital Sky Survey to estimate the fraction of local star formation as a function of host galaxy oxygen abundance. We find that only a small fraction ( < 25%) of current star formation occurs in galaxies with oxygen abundance 12 + log (O/H) < 8.6, i.e., about half that of the Milky Way. However, all five low-z GRB hosts have oxygen abundance below this limit, in three cases very significantly so. If GRBs traced local star formation independent of metallicity, the probability of obtaining such low abundances for all five hosts would be p approximate to 0.1%. We conclude that GRBs trace only low-metallicity star formation, and that the Milky Way has been too metal rich to host long GRBs for at least the last several billion years. This result has implications for the potential role of GRBs in mass extinctions, for searches for recent burst remnants in the Milky Way and other large galaxies, for non-detections of late radio emission from local core-collapse supernovae, and for the production of cosmic rays in the local Universe. Our results agree with theoretical models that tic GRBs to rapidly spinning progenitors, which require minimal angular momentum loss in stellar winds. We also find that the isotropic energy release of these five GRBs, E-iso, steeply decreases with increasing host oxygen abundance. This might further indicate that (low) metallicity plays a fundamental physical role in the GRB phenomenon, and suggesting an upper metallicity limit for "cosmological" GRBs at approximate to 0.15 Z((.)). C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stanek, KZ (reprint author), Ohio State Univ, Dept Astron, 174 W 18th Ave, Columbus, OH 43210 USA. EM kstanek@astronomy.ohio-state.edu; ognedin@astronomy.ohio-state.edu; beacom@mps.ohio-state.edu; gould@astronomy.ohio-state.edu; jaj@astronomy.ohio-state.edu; jak@astronomy.ohio-state.edu; mmodjaz@cfa.harvard.edu; pinsono@astronomy.ohio-state.edu; pogge@astronomy.ohio-state.edu; dhw@astronomy.ohio-state.edu OI Beacom, John/0000-0002-0005-2631 NR 55 TC 159 Z9 160 U1 0 U2 6 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2006 VL 56 IS 4 BP 333 EP 345 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129NE UT WOS:000243735400003 ER PT J AU Barnett, AA Sampaio, EM Kalko, EK Shapley, RL Fisher, E Camargo, G Rodriguez-Herrera, B AF Barnett, Adrian A. Sampaio, Erica M. Kalko, Elisabeth K. V. Shapley, Rebecca L. Fisher, Erich Camargo, George Rodriguez-Herrera, Bernal TI Bats of Jau National Park, central Amazonia, Brazil SO ACTA CHIROPTEROLOGICA LA English DT Review DE Amazonia; inventory; bats; ecology; conservation ID FRUIT-EATING BATS; CAROLLIA-PERSPICILLATA CHIROPTERA; LOWLAND RAIN-FOREST; FRENCH-GUIANA; SPECIES RICHNESS; FORAGING BEHAVIOR; FLORISTIC COMPOSITION; NOCTILIO-ALBIVENTRIS; POLLINATION BIOLOGY; COMMUNITY STRUCTURE AB Although recognized as highly diverse. the bat fauna of the Amazon basin has been only patchily sampled. This paper combines data from five short surveys conducted between 1998 and 2001 in Jail National Park. 220 kill east of Manaus central Amazonia. We used mist-nets. recordings of echolocation calls and roost visits to provide the first bat inventory for this area. A total of 53 bat species in 33 genera and five families were documented, including several species that are regarded as rare, in particular Saccopteryx gymnura, Vampyriscus brocki, Molossops neglectus, and Promops centralis. The Chao 1 index indicates that sampling is about 72% complete, suggesting that around 73 bat species might co-exist in Jau. We compare the composition of Jau's bat fauna to those of other sites in Amazonia and interpret the resulting patterns of diversity. Data on reproduction are given for 14 species. C1 Akodon Ecol Consulting, Concord, CA 94518 USA. Roehampton Univ, Sch Life Sci, Ctr Res Evolutionary Anthropol, London SW15 3SN, England. Smithsonian Inst, NMNH, Div Mammals, Washington, DC 20560 USA. Univ Ulm, Dept Expt Ecol, Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. Univ Fed Mato Grosso do Sul, Dept Biol, BR-79070900 Campo Grande, MS, Brazil. Museo Nacl Costa Rica, San Jose 7491000, Costa Rica. RP Barnett, AA (reprint author), Akodon Ecol Consulting, 951 Bancroft Rd,Suite 111A, Concord, CA 94518 USA. EM adrian@akodon.com OI Fischer, Erich/0000-0001-8722-9876 NR 120 TC 15 Z9 18 U1 2 U2 13 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2006 VL 8 IS 1 BP 103 EP 128 DI 10.3161/1733-5329(2006)8[103:BOJNPC]2.0.CO;2 PG 26 WC Zoology SC Zoology GA 048FN UT WOS:000237933100008 ER PT J AU Dietz, M Encarnacao, JA Kalko, EKV AF Dietz, Markus Encarnacao, Jorge A. Kalko, Elisabeth K. V. TI Small scale distribution patterns of female and male Daubenton's bats (Myotis daubentonii) SO ACTA CHIROPTEROLOGICA LA English DT Article DE Myotis daubentonii; sex ratio; abundance; distribution; conservation ID INSECTIVOROUS BAT; FORAGING BEHAVIOR; BROWN BATS; VESPERTILIONIDAE; CHIROPTERA; ECHOLOCATION; LUCIFUGUS; HABITAT; ECOLOGY; TORPOR AB We analysed the distribution and relative abundance of Myotis daubentonii in the lowlands and uplands around the Lahn river near the city of Giessen (Hessen, Central Germany). We assumed a positive correlation between distribution and relative abundance of the trawling M. daubentonii with the amount of water surface in our study area. We further expected an unequal distribution of male and female M. daubentonii especially during the energy demanding pregnancy and lactation period of females. Daubenton's bats were found at 75% of the 64 ponds and lakes we surveyed by standardized nightly spotlight counts. The number of Daubenton's bats correlated positively with the area of the water surface and negatively with the distance to the nursery colonies. Nursery colonies were located with radio-tracking and existed predominantly in the lowlands close to the Lahn river. Mean flight distance between nursery colonies and foraging areas was 2.3 km (mean +/- 1.4 km, range: 0.6-6.3 km). Sex ratio was determined at three sites studied in detail from 1992-2003 by mist-netting along regular used flight paths (n = 1,847 caught individuals). The number of female per male M. daubentonii was unequal and differed significantly between the three sites. In the lowland we found one site clearly dominated by females (median = 4.3 females per male, percentages of females 79.3%, n 169 individuals) and a second site with an almost balanced sex ratio (median = 1.1 females per male, percentages of females 50.3%, n = 939 individuals). At the third site in the uplands males outnumbered females (median = 0.2 females per male, percentages of females 13.5%, n = 739 individuals). The percentages of females remained largely constant from spring to mid summer and changed at the beginning of September. The study revealed that a detailed knowledge of the spatial distribution of gender specific roost sites and key foraging habitats is necessary for the establishment of meaningful monitoring and conservation measures for bats. C1 Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Univ Giessen, Dept Anim Ecol, D-35392 Giessen, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Dietz, M (reprint author), Univ Ulm, Dept Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM Markus.Dietz@tieroekologie.com NR 52 TC 28 Z9 30 U1 2 U2 19 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 EI 1733-5329 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2006 VL 8 IS 2 BP 403 EP 415 DI 10.3161/1733-5329(2006)8[403:SSDPOF]2.0.CO;2 PG 13 WC Zoology SC Zoology GA 126GK UT WOS:000243500500007 ER PT J AU Ortega, J Maldonado, JE AF Ortega, Jorge Maldonado, Jesus E. TI Female interactions in harem groups of the Jamaican fruit-eating bat, Artibeus jamaicensis (Chiroptera : Phyllostomidae) SO ACTA CHIROPTEROLOGICA LA English DT Article DE aggressive interactions; affiliative interactions; Artibeus jamaicensis; harem groups ID SOCIAL-ORGANIZATION; VAMPIRE BAT; CAVE BATS; BEHAVIOR; VESPERTILIONIDAE; ASSOCIATION; COLONIES; DEFENSE; MEXICO; MALES AB Harem groups of the Jamaican fruit-eating bat (Artibeus jamaicensis) are well-defined units that occupy different crevices in caves. For two consecutive years, we analyzed the non-random associations among female bats and their interactions with other members of the harem. Female members occupying the edges of the harems came from different parts of the cave and were more frequently expelled from the roosting site. Females from the central core of the harem were attacked less often and received more affiliative interactions. Females occupying areas between the central core and the edges were the most active in repelling arriving females and were responsible for grooming the central core females. During the breeding season, aggressive activities decreased and females became more tolerant, which suggests that a potential benefit of roosting together is that it provides for a more suitable place to nurse newborns, because all females produce a better environment, in thermoregulatory ways. C1 Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Biodiversidad, Lab Macroecol, Mexico City 04510, DF, Mexico. Smithsonian Inst, Natl Zool Pk, Genet Program, Natl Museum Nat Hist, Washington, DC 20008 USA. RP Ortega, J (reprint author), Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Biodiversidad, Lab Macroecol, AP 70-245,Circuito Exterior Junto Jardin Bot,Ciud, Mexico City 04510, DF, Mexico. EM artibeus2@aol.com NR 38 TC 12 Z9 13 U1 1 U2 11 PU POLISH ACAD OF SCIENCES PI WARSAW PA MUSEUM & INST ZOOLOGY WILCZA 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2006 VL 8 IS 2 BP 485 EP 495 DI 10.3161/1733-5329(2006)8[485:FIIHGO]2.0.CO;2 PG 11 WC Zoology SC Zoology GA 126GK UT WOS:000243500500015 ER PT S AU Goddard, I AF Goddard, Ives BE Wolfart, HC TI The Proto-Algonquian negative and its descendants SO ACTES DU TRENTE-SEPTIEME CONGRES DES ALGONIQUINISTES SE Papers of the Algonquin Conference LA English DT Proceedings Paper CT 37th Algonquian Conference CY OCT 21-23, 2005 CL Univ Carleton, Canadian Museum Civilisat, Quebec, CANADA HO Univ Carleton, Canadian Museum Civilisat ID MESKWAKI; CREE C1 Smithsonian Inst, Washington, DC 20560 USA. NR 77 TC 2 Z9 2 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA SN 0831-5671 J9 PAP ALGON CONF PY 2006 VL 37 BP 161 EP 208 PG 48 WC Linguistics SC Linguistics GA BGQ96 UT WOS:000249887800009 ER PT J AU Wen, J Lowry, PP AF Wen, Jun Lowry, Porter P., II TI New species and new combinations in Brassaiopsis (Araliaceae) from Vietnam and southwestern China SO ADANSONIA LA English DT Article DE Acanthopanax; Araliaceae; Brassaiopsis; China; Vietnam; new species ID SEQUENCES; NUCLEAR AB BrassaiopsisficifolioidesJ.Wen & Lowry (Araliaceae) is described based on material in the Paris herbarium from Lao Cai Province, northern Vietnam, previously associated with another well delimited species, A ficifolia Dunn. Brassaiopsis gigantea J.Wen & Lowry is described from Ninh Binh Province, north-central Vietnam, based on collections from Cuc Phuong National Park. Recent field work has shown that Acanthopanax bodinieri H.Lev. from southwestern China and northern Vietnam, long regarded as a synonym of B. ciliata Dunn, also represents a distinct species, necessitating its transfer to Brassaiopsis. Another taxon, previously described as B. ficifolia var. nhatrangensis Bui from southern Vietnam, is likewise distinct, and is thus also elevated to the rank of species. C1 Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. Chinese Acad Sci, Inst Bot, Lab Syst & Evolutionary Bot, Beijing 100093, Peoples R China. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Missouri Bot Garden, St Louis, MO 63166 USA. Museum Natl Hist Nat, Dept Syst & Evolut, UMS 602, F-75231 Paris 05, France. RP Wen, J (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166,POB 37012, Washington, DC 20013 USA. EM wenj@si.edu; lowry@mnhn.fr NR 8 TC 1 Z9 1 U1 0 U2 1 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-8571 J9 ADANSONIA JI Adansonia PY 2006 VL 28 IS 1 BP 181 EP 190 PG 10 WC Plant Sciences SC Plant Sciences GA 082TU UT WOS:000240410900017 ER PT S AU Kramer, EM Zimmer, EA AF Kramer, Elena M. Zimmer, Elizabeth A. BE Soltis, DE LeebensMack, JH Soltis, PS Callow, JA TI Gene duplication and floral developmental genetics of basal eudicots SO ADVANCES IN BOTANICAL RESEARCH: INCORPORATING ADVANCES IN PLANT PATHOLOGY, VOL 44: DEVELOPMENTAL GENETICS OF THE FLOWER SE Advances in Botanical Research LA English DT Review; Book Chapter ID MADS-BOX GENE; ESCHSCHOLZIA-CALIFORNICA CHAM.; CONTROLLING FLOWER DEVELOPMENT; HOMEOTIC PROTEINS APETALA1; TERNARY COMPLEX-FORMATION; ORGAN-IDENTITY PROTEINS; ARABIDOPSIS-THALIANA; MERISTEM IDENTITY; ANTIRRHINUM-MAJUS; CLASS-B AB The diversification of floral morphology is likely to be due to multiple independent changes in many different components of the genetic pathways that control floral development. One of the best-understood participants in this developmental process is the floral organ identity program. Although many fundamental aspects of this program are conserved within angiosperms and even seed plants, significant developmental system drift has occurred, often in association with gene duplication events. In this review, we consider the many gene duplications that have been identified within the basal eudicot grade, a group of lineages which represent a critical stage of angiosperm evolution. These events are of particular interest since they appear to have laid the foundation for the canonical ABC-model that has been described in the core eudicots. Furthermore, the frequent occurrence of gene duplication in floral organ identity gene lineages offers an excellent opportunity to study the effects of processes, such as neo- and subfunctionalization, on a preexisting genetic program. C1 Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Suitland, MD 20746 USA. Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA. RP Kramer, EM (reprint author), Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA. RI Zimmer, Elizabeth/G-3890-2011; Soltis, Pamela/L-5184-2015 NR 137 TC 15 Z9 15 U1 0 U2 12 PU ACADEMIC PRESS LTD-ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL ROAD, LONDON NW1 7DX, ENGLAND SN 0065-2296 BN 978-0-12-005944-7 J9 ADV BOT RES JI Adv. Bot. Res. PY 2006 VL 44 BP 353 EP 384 DI 10.1016/S0065-2296(06)44009-X PG 32 WC Plant Sciences SC Plant Sciences GA BFT61 UT WOS:000244525100009 ER PT J AU Bemporad, A Poletto, G Raymond, JC AF Bemporad, A. Poletto, G. Raymond, J. C. TI Evidence for pyroxene dust grains in C/2001 C2 sungrazing comet SO ADVANCES IN SPACE RESEARCH LA English DT Article DE comets; general; comets; individual (C/2001 C2); spectroscopy; EUV ID SOLAR; COLLISIONS; UVCS AB In this paper we analyze SOHO/UVCS data of the sungrazing comet C/2001 C2, a member of the Kreutz family, that was observed on February 7, 2001, at the beliocentric distances of 4.98 and 3.60 solar radii. This comet splits in a main nucleus and a fragment which have been identified in UV data. A study of the cometary Hydrogen Ly alpha emission from these two objects revealed that the Ly alpha signal from the fragment decays exponentially with time, while the signal from the main object consists of an exponentially decaying term superposed onto a constant background. The latter emission has been ascribed to the sublimation of pyroxene dust grains, whose end products neutralize coronal protons via charge exchange processes. This interpretation allowed us to estimate, for the first time, the number density of pyroxene dust grains in a sungrazing comet. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bemporad, A.] Univ Florence, Dept Astron, I-50125 Florence, Italy. [Poletto, G.] INAF Arcetri Astrophys Observ, I-50125 Florence, Italy. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bemporad, A (reprint author), Univ Florence, Dept Astron, Lgo E Fermi 2, I-50125 Florence, Italy. EM bemporad@arcetri.astro.it; pole-tto@arcetri.astro.it; jraymond@cfa.harvard.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 9 BP 1972 EP 1975 DI 10.1016/j.asr.2005.10.005 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600013 ER PT J AU Munoz-Darias, T Martinez-Paris, IG Casares, J Marsh, TR Cornelisse, R Steeghs, D Dhillon, VS Charles, PA AF Munoz-Darias, T. Martinez-Paris, I. G. Casares, J. Marsh, T. R. Cornelisse, R. Steeghs, D. Dhillon, V. S. Charles, P. A. TI Multiband echo tomography of Sco X-1 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE binaries : close; X-rays : binaries; stars : individual : Sco X-1 ID MASS AB We present preliminary results of a simultaneous X-ray/optical campaign of the prototypical LMXB Sco X-1 at 1-10 Hz time resolution. Lightcurves of the high excitation Bowen/Hell emission lines and a red continuum at lambda(c) similar to 6000 angstrom were obtained through narrow interference filters with ULTRACAM, and these were cross-correlated with simultaneous RXTE X-ray lightcurves. We find evidence for correlated variability, in particular when Sco X-1 enters the Flaring branch. The Bowen/Hell lightcurves lag the X-ray lightcurves with a light travel time which is consistent with reprocessing in the companion star while the continuum lightcurves have shorter delays consistent with reprocessing in the accretion disc. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Munoz-Darias, T.; Martinez-Paris, I. G.; Casares, J.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Cornelisse, R.; Charles, P. A.] Sch Phys & Astron, Southampton SOB17 1BJ, Hants, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dhillon, V. S.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Charles, P. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Munoz-Darias, T (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. EM tmd@iac.es RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 5 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2762 EP 2764 DI 10.1016/j.asr.2005.10.056 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900020 ER PT J AU Mukhopadhyay, B Afshordi, N Narayan, R AF Mukhopadhyay, Banibrata Afshordi, Niayesh Narayan, Ramesh TI Growth of hydrodynamic perturbations in accretion disks: Possible route to non-magnetic turbulence SO ADVANCES IN SPACE RESEARCH LA English DT Article DE accretion; accretion disk; hydrodynamic; turbulence; instabilities ID INSTABILITY; STABILITY; TRANSPORT; BYPASS; FLOW AB We study the possible origin of hydrodynamic turbulence in cold accretion disks such as those in star-forming systems and quiescent cataclysmic variables. As these systems are expected to have neutral gas, the turbulent viscosity is likely to be hydrodynamic in origin, not magnetohydrodynamic. Therefore, MRI will be sluggish or even absent in such disks. Although there are no exponentially growing eigenmodes in a hydrodynamic disk because of the non-normal nature of the eigenmodes, a large transient growth in the energy is still possible, which may enable the system to switch to a turbulent state. For a Keplerian disk, we estimate that the energy will grow by a factor of 1000 for a Reynolds number close to a million. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Mukhopadhyay, Banibrata; Afshordi, Niayesh; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Mukhopadhyay, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM bmukhopa@cfa.harvard.edu NR 13 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2877 EP 2879 DI 10.1016/j.asr.2005.09.048 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900048 ER PT J AU Grindlay, JE AF Grindlay, Jonathan E. TI Compact X-ray binaries in and out of core collapsed globulars SO ADVANCES IN SPACE RESEARCH LA English DT Article DE globular clusters; X-rays, general; binaries, close, cataclysmic variables, X-ray binaries, millisecond pulsars ID CLUSTER NGC-6397; CATACLYSMIC VARIABLES; GLOBULAR-CLUSTER-47 TUCANAE; MILLISECOND PULSARS; CHANDRA; IDENTIFICATION; POPULATION; CATALOG; STARS; 47TUC AB We review new Chandra and HST observations of the core collapsed cluster NGC 6397 as a guide to understanding the compact binary (CB) populations in core collapse globulars. New cataclysmic variables (M) and main sequence chromospherically active binaries (ABs) have been identified, enabling a larger sample for comparison of the L(x), F(x)/F(V), and X-ray vs. optical color distributions. Comparison of the numbers of CBs with L(x) greater than or similar to 10(31) erg s(-1) in 4 core collapse vs. 12 King model clusters reveals that the specific frequency S(X) (number of CBs per unit cluster mass) is enhanced in core collapse Clusters, even when normalized for their stellar encounter rate. Although core collapse is halted by the dynamical heating due to stellar (and binary) interaction with CBs in the core, we conclude that production of the hardest CBs - especially CVs - is enhanced during core collapse. NGC 6397 has its most luminous CVs nearest the cluster center, with two newly discovered very low luminosity (old, quiescent) CVs far from the core. The active binaries as well as neutron star systems (MSP and qLMXB) surround the central core. The overall CB population appears to be asymmetric about the cluster center, as in several other core collapse clusters observed with Chandra, suggesting still poorly understood scattering processes. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. 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 20 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2923 EP 2929 DI 10.1016/j.asr.2006.04.027 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900060 ER PT J AU Fabbiano, G AF Fabbiano, G. TI X-ray populations in galaxies SO ADVANCES IN SPACE RESEARCH LA English DT Article DE astrophysics; X-ray sources; Chandra; X-ray luminosity functions (XLFs) ID MULTIVARIATE STATISTICAL-ANALYSIS; LUMINOSITY FUNCTION; CHANDRA OBSERVATIONS; SPECTRAL PROPERTIES; STAR-FORMATION; POINT SOURCES; BINARIES; ANTENNAE; EMISSION; INDICATOR AB High-resolution Chandra observations have allowed the detection of populations of X-ray sources in galaxies of all morphological types. The X-ray Luminosity Functions (XLFs) of these X-ray source populations have been derived and studied to uncover the drivers for the formation and evolution of binaries in different stellar populations and environments. These XLFs also provide a tool for identifying the nature of the X-ray source Population, since different XLFs characterize X-ray sources belonging to young and old stellar populations. Similarly, X-ray colors can be used for identifying different types of X-ray sources. Ultra-Luminous X-ray sources (ULXs, L(X) > 10(39) ergs s(-1)) are found to be associated with star-forming stellar populations. The study of the ULX population of the Antennae galaxies points to compact accreting binaries. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pepi@cfa.harvard.edu NR 31 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2937 EP 2941 DI 10.1016/j.asr.2006.04.033 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900062 ER PT J AU Kim, DW AF Kim, Dong-Woo TI LMXB luminosity function and connection to globular cluster in early type galaxies SO ADVANCES IN SPACE RESEARCH LA English DT Article DE early type galaxies; X-ray; LMXB; globular clusters ID X-RAY BINARIES; ELLIPTIC GALAXIES; CHANDRA OBSERVATIONS; SOURCE POPULATION; MASS; STAR; MULTIWAVELENGTH; INDICATOR AB We derive bias-corrected X-ray luminosity functions (XLFs) of LMXBs detected in 14 E and S0 galaxies observed with Chandra. After correcting for incompleteness, the individual XLFs are statistically consistent with a single power-law. A break at or near L(X.Eddington), as previously reported, is not required in any individual case. The combined XLF with a reduced error, however, suggests a possible break at L(X) = 5 x 10(38) erg s(-1), which may be consistent with the Eddington luminosity of neutron stars with the largest possible mass (3 M(circle dot)), or of He-enriched neutron star binaries. We confirm that the total X-ray luminosity of LMXBs is correlated with the the near-IR luminosities, but the scatter exceeds that expected from measurement errors. The scatter in L(X)(LMXB)/L(K) appears to be correlated with the specific frequency of globular clusters, as reported earlier. We cross-correlate X-ray binaries with globular clusters determined by ground-based optical and HST observations in 6 giant elliptical galaxies. With the largest sample reported so far (similar to 300 GC LMXBs with a 5:2 ratio between red and blue GCs), we compare their X-ray properties. such as X-ray hardness, XLF and L(X)/L(B) and find no statistically significance difference between different groups of LMXBs. Regardless of their association with GCs, both GC and field LMXBs appear to follow the radial profile of the optical halo light, rather than that of more extended GCs. This suggests that while metallicity is a primary factor in the formation of LMXBs in GCs, there may be a secondary factor (e.g., encounter rate) playing a non-negligible role. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM kim@cfa.harvard.edu NR 30 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2942 EP 2945 DI 10.1016/j.asr.2006.03.043 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900063 ER PT J AU Zezas, A AF Zezas, Andreas TI X-ray source populations in nearby star-forming galaxies SO ADVANCES IN SPACE RESEARCH LA English DT Article AB We present results on the X-ray source populations of nearby star-forming galaxies based on Chandra observations. First we discuss the monitoring, campaigns on the Antennae and M82 galaxies. In both cases we find that the majority of the X-ray sources exhibit intensity and/or spectral variability. However, despite of this variability, we do not find any statistically significant variations of their X-ray luminosity functions (XLFs). We also find that the majority of the X-ray sources are associated with star-forming regions, although we do not always identify optical counterparts to the X-ray sources. Especially in the case of M82 we find that the most luminous sources are clustered in the central region of the galaxy. Finally, we present the first results from a study of a sample of nearby star-forming galaxies which form a starburst age sequence: although their XLFs to first order are represented by power-laws with consistent slopes, there is an indication for small variations, suggesting a change of their X-ray binary populations. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM azezas@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 8 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2946 EP 2949 DI 10.1016/j.asr.2006.02.070 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900064 ER PT J AU Crouch, T AF Crouch, T TI Looking forward ... looking back SO AEROSPACE AMERICA LA English DT Editorial Material C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, T (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD JAN PY 2006 VL 44 IS 1 BP 3 EP 3 PG 1 WC Engineering, Aerospace SC Engineering GA 000YV UT WOS:000234499400001 ER PT J AU Joynes, SN AF Joynes, SN TI "Indian" stereotypes in TV science fiction: First nations' voices speak out. SO AMERICAN INDIAN CULTURE AND RESEARCH JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Resource Ctr, New York, NY 10004 USA. RP Joynes, SN (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Resource Ctr, 1 Bowling Green, New York, NY 10004 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU U C L A, AMER INDIAN STUDIES CENTER PI LOS ANGELES PA 3220 CAMPBELL HALL, BOX 951548, LOS ANGELES, CA 90095-1548 USA SN 0161-6463 J9 AM INDIAN CULT RES J JI Am. Indian Cult. Res. J. PY 2006 VL 30 IS 1 BP 151 EP 153 PG 3 WC History SC History GA 057IK UT WOS:000238589300017 ER PT J AU Chiu, CH Bajwa, T Homiski, R Potts, R AF Chiu, CH Bajwa, T Homiski, R Potts, R TI Environmental dynamics on an evolutionary time scale can shape the genetic basis of an organism's adaptability: Insights from the mighty worm (C-elegans) SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Rutgers State Univ, Dept Genet, Piscataway, NJ 08855 USA. Rutgers State Univ, Ctr human Evolutionary Studies, Dept Anthropol, Piscataway, NJ 08855 USA. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2006 SU 42 BP 75 EP 75 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 016YQ UT WOS:000235661100082 ER PT J AU Meier, LN Hunt, DR AF Meier, LN Hunt, DR TI Incidence of humeral septal aperture and its relation to population and sex. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 2 Z9 3 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2006 SU 42 BP 129 EP 129 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 016YQ UT WOS:000235661100305 ER PT J AU Mulhern, DM Ubelaker, DH AF Mulhern, DM Ubelaker, DH TI Bone microstructure in chimpanzees. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Ft Lewis Coll, Dept Anthropol, Durango, CO 81301 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2006 SU 42 BP 135 EP 135 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 016YQ UT WOS:000235661100330 ER PT J AU Ousley, SD Hollinger, RE Utermohle, CJ AF Ousley, SD Hollinger, RE Utermohle, CJ TI Northern Arctic population structure, history, and migrations in light of new data and methods. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Alaska Dept Hlth & Social Serv, Anchorage, AK USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2006 SU 42 BP 142 EP 143 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 016YQ UT WOS:000235661100360 ER PT J AU Phelps, SM Rand, AS Ryan, MJ AF Phelps, SM Rand, AS Ryan, MJ TI A cognitive framework for mate choice and species recognition SO AMERICAN NATURALIST LA English DT Article DE mate choice; sexual selection; animal communication; animal cognition; decision theory; perceptual error ID FEMALE MATING PREFERENCES; SEXUAL SELECTION; PHYSALAEMUS-PUSTULOSUS; TUNGARA FROGS; ANIMAL COMMUNICATION; PATTERN-RECOGNITION; CALL PREFERENCES; TREEFROGS ANURA; NEURAL-NETWORKS; MODELS AB Mating decisions contribute to both the fitness of individuals and the emergence of evolutionary diversity, yet little is known about their cognitive architecture. We propose a simple model that describes how preferences are translated into decisions and how seemingly disparate patterns of preference can emerge from a single perceptual process. The model proposes that females use error-prone estimates of attractiveness to select mates based on a simple decision rule: choose the most attractive available male that exceeds some minimal criterion. We test the model in the tungara frog, a well-characterized species with an apparent dissociation between mechanisms of mate choice and species recognition. As suggested by our model results, we find that a mate attraction feature alters assessments of species status. Next, we compare female preferences in one-choice and two-choice tests, contexts thought to emphasize species recognition and mate choice, respectively. To do so, we use the model to generate maximum-likelihood estimators of preference strengths from empirical data. We find that a single representation of preferences is sufficient to explain response probabilities in both contexts across a wide range of stimuli. In this species, mate choice and species recognition are accurately and simply summarized by our model. While the findings resolve long-standing anomalies, they also illustrate how models of choice can bridge theoretical and empirical treatments of animal decisions. The data demonstrate a remarkable congruity of perceptual processes across contexts, tasks, and taxa. C1 Univ Florida, Dept Zool, Gainesville, FL 32605 USA. Smithsonian Inst, Smithsonian Trop Res Inst, Gamboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RP Phelps, SM (reprint author), Univ Florida, Dept Zool, B30 Bartram Hall, Gainesville, FL 32605 USA. EM phelps@zoo.ufl.edu NR 44 TC 52 Z9 53 U1 4 U2 26 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD JAN PY 2006 VL 167 IS 1 BP 28 EP 42 DI 10.1086/498538 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 998AD UT WOS:000234289300004 PM 16475097 ER PT J AU Archie, EA Morrison, TA Foley, CAH Moss, CJ Alberts, SC AF Archie, EA Morrison, TA Foley, CAH Moss, CJ Alberts, SC TI Dominance rank relationships among wild female African elephants, Loxodonta africana SO ANIMAL BEHAVIOUR LA English DT Article ID RED DEER HINDS; REPRODUCTIVE SUCCESS; SOCIAL-DOMINANCE; EGALITARIAN SOCIETIES; ASSOCIATION PATTERNS; SPIDER MONKEYS; MOUNTAIN GOATS; EAST-AFRICA; HIERARCHIES; POPULATION AB Socioecological models of the evolution of female-bonded societies predict a relation between resource distribution and the nature of female affiliative and dominance relationships. Species that mainly rely on abundant, widely distributed resources, like African savanna elephants, are predicted to have unresolved dominance hierarchies and poorly differentiated female social relationships. Contrary to this prediction, female elephants have well-differentiated social relationships; however, little is known about the nature of their dominance rank relationships. Here we present the first quantitative analysis of dominance relationships within 'family' groups of adult female elephants in two wild populations: one in Amboseli National Park, Kenya, and another in Tarangire National Park, Tanzania. We tested three possibilities, that female elephants: (1) are egalitarian, (2) have linear, nepotistic hierarchies, or (3) have linear age/size-ordered hierarchies. Our results best support the third outcome: dominance rank relationships were transitive within families and highly asymmetrical within dyads, such that older, larger females consistently dominated smaller, younger females. We discuss the implications of this result for understanding the evolution of female social relationships. (c) 2005 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Duke Univ, Dept Biol, Durham, NC 27706 USA. Tarangire Elephant Project, Arusha, Tanzania. Amboseli Elephant Res Project, Nairobi, Kenya. RP Archie, EA (reprint author), Natl Museum Nat Hist, Smithsonian Genet Program, 3001 Connecticut Ave,NW, Washington, DC 20008 USA. EM archiee@si.edu NR 86 TC 90 Z9 92 U1 3 U2 88 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 JAN PY 2006 VL 71 BP 117 EP 127 DI 10.1016/j.anbehav.2005.03.023 PN 1 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 004PK UT WOS:000234764500012 ER PT J AU Srygley, RB Dudley, R Oliveira, EG Riveros, AJ AF Srygley, RB Dudley, R Oliveira, EG Riveros, AJ TI Experimental evidence for a magnetic sense in Neotropical migrating butterflies (Lepidoptera : Pieridae) SO ANIMAL BEHAVIOUR LA English DT Article ID SPINY LOBSTERS; COIL SYSTEMS; ORIENTATION; FIELD; HONEYBEES; COMPASS; LIGHT; CALIBRATION; MECHANISMS; TENEBRIO AB We tested whether migrating Aphrissa statira butterflies orient with a magnetic compass. We captured migrants flying over Lake Gatun, Panama, and exposed experimental butterflies to a strong magnetic field. These and unmanipulated control butterflies were released back over the lake. Experimental butterflies had a more dispersed pattern of orientation than control butterflies. The average direction adopted was northeast, 160 degrees anticlockwise to the natural migratory direction. Unmanipulated control butterflies adopted two diametrically opposed orientations: one shifted 33 degrees clockwise, and another 147 degrees anticlockwise, to the migratory direction. Control and experimental butterflies differed in that some controls oriented towards the migratory direction. These differences in orientation support the hypothesis of a sense for magnetic orientation cues. Unmanipulated butterflies released over the lake when the sky was completely overcast were significantly oriented towards their direction before capture (187 degrees and 203 degrees, respectively), further supporting the magnetic compass hypothesis. In a third experiment, we obstructed sun compass cues and reversed the horizontal component of the local geomagnetic field to position magnetic north towards the geographical south pole within a flight arena into which we released individual butterflies. Experimental butterflies experiencing the reversed magnetic field oriented on average 180 degrees opposite to their natural migratory direction. Control butterflies, for which the position of magnetic north was unaltered, were oriented both towards and 180 degrees opposite to the natural migratory direction. This difference between orientations of control and experimental butterflies also supports the hypothesis of a sense for magnetic orientation cues. (c) 2005 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Oxford, Dept Zool, Oxford OX1 3PS, England. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Univ Fed Minas Gerais, Dept Biol Geral, BR-30161970 Belo Horizonte, MG, Brazil. Univ Nacl Colombia, Dept Biol, Bogota, Colombia. RP Srygley, RB (reprint author), Smithsonian Trop Res Inst, Apdo 2072, Balboa, Panama. EM bob.srygley@zoo.ox.ac.uk NR 39 TC 17 Z9 23 U1 1 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 JAN PY 2006 VL 71 BP 183 EP 191 DI 10.1016/j.anbehav.2005.04.013 PN 1 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 004PK UT WOS:000234764500019 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI A review of the new world species of the shore-fly genus Leptopsilopa Cresson (Diptera : Ephydridae) SO ANNALES ZOOLOGICI LA English DT Article DE shore flies; Ephydridae; Leptopsilopa; review; New World AB The 12 New World species of Leptopsilopa are reviewed, including the following new species (type localities noted parenthetically): L. andiana (Peru. Huanuco: Espensa, [ 11 km N Hudinico]), L. flavicoxa (Belize. Stann Creek: Cockscomb Basin Wildlife Sanctuary [16 degrees 47'N, 88 degrees 30'W]), L. martharum (United States. Texas. Jim Wells: Mathis (7.5 km S; Nueces River; 28 degrees 02.2'N, 97 degrees 52.2'W; 15 m), and L. placentia (Belize. Stann Creek-Placentia Lagoon, Rum Point; 16 degrees 32'N, 88 degrees 21'W). Lectotypes are designated for Psilopa similis Coquillett, Psilopa varipes Coquillett, and Psilopa metallina Becker. The monophyly of Leptopsilopa is established, but only if the Old World species are excluded. The genus is most closely related to a lineage of species currently included in the genus Psilopa (the dupla group, including R metallina), which is rendered paraphyletic by the recognition of Leptopsilopa as an included, monophyletic lineage. The New World species are arranged into two monophyletic species groups, the atrimana and the similis groups. Of the 12 species now recognized, 10 occur in the neotropics, where other undescribed species will probably be discovered. C1 Smithsonian Inst, Washington, DC 20013 USA. Univ Opole, Dept Biosystemat, PL-45052 Opole, Poland. EM mathisw@si.edu; zatwar@uni.opole.pl OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 43 TC 2 Z9 3 U1 0 U2 0 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 0003-4541 J9 ANN ZOOL JI Ann. Zool. PY 2006 VL 56 IS 1 BP 85 EP 138 PG 54 WC Entomology SC Entomology GA 033UP UT WOS:000236876000007 ER PT J AU Sakai, AK Weller, SG Wagner, WL Nepokroeff, M Culley, TM AF Sakai, Ann K. Weller, Stephen G. Wagner, Warren L. Nepokroeff, Molly Culley, Theresa M. TI Adaptive radiation and evolution of breeding systems in Schiedea (Caryophyllaceae), an endemic Hawaiian genus SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article; Proceedings Paper CT 50th Annual Systematics Symposium of the Missouri-Botanical-Garden CY OCT 10-11, 2003 CL Missouri Bot Garden, St Louis, MO HO Missouri Bot Garden DE adaptive radiation; autogamy; breeding systems; Hawaii; inbreeding depression; resource allocation; Schiedea; selfing; sexual dimorphism ID SPERGULARIA-MARINA CARYOPHYLLACEAE; SILENE-LATIFOLIA CARYOPHYLLACEAE; FLORAL TRAITS; QUANTITATIVE GENETICS; INBREEDING DEPRESSION; SEXUAL-DIMORPHISM; ALSINIDENDRON CARYOPHYLLACEAE; FLOWERING PLANTS; SALICARIA CARYOPHYLLACEAE; LYDGATEI CARYOPHYLLACEAE AB A multi-disciplinary approach, including phylogenetic analysis, population biology, and quantitative genetics, has helped to elucidate the selective factors that have promoted speciation and shifts in breeding systems in Schiedea (Caryophyllaccae). Schiedea is the fifth largest lineage in the native Hawaiian flora and the most diverse lineage with respect to breeding systems. The genus is monophyletic and shares a common ancestor with a clade consisting of two arctic or boreal-north temperate species. Most inter-island colonizations were from older to younger islands, and most movement between islands led to sufficient isolation to result in formation of new species that are single-island endemics rather than species with multi-island distributions. Closely related species pairs occuring on older islands tend to differ in habitat and are isolated ecologically on the same island, while species pairs on younger islands tend to be in similar habitat on different islands. Speciation within this lineage has been associated with shifts in habitat, pollination system, and breeding system, including evolution of selfing (obligate autogamy, faculatative autogamy), mixed mating systems, and dimorphism (gynodioecy, subdioecy, and dioecy). Dimorphic breeding systems appear to have been derived independently twice in Schiedea, and facultative autogamy and obligate autogamy have both evolved three times. The colonization of windy, dry habitats appears to occur before changes in sex allocation patterns. and the evolution of dimorphism in this lineage has been promoted by the combination of high inbreeding depression and high selfing rates. Many morphological traits associated with allocation to male and female function are highly heritable, and genetic correlations in general do not appear to constrain the evolulion of dimorphism in Schiedea. C1 Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. Univ Cincinnati, Dept Biol Sci, Cincinnati, OH 45221 USA. RP Sakai, AK (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. NR 81 TC 39 Z9 40 U1 6 U2 29 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2006 VL 93 IS 1 BP 49 EP 63 DI 10.3417/0026-6493(2006)93[49:ARAEOB]2.0.CO;2 PG 15 WC Plant Sciences SC Plant Sciences GA 050VX UT WOS:000238118300006 ER PT J AU Piperno, DR AF Piperno, Dolores R. TI Quaternary environmental history and agricultural impact on vegetation in Central America SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article; Proceedings Paper CT 51st Annual Systematics Symposium of the Missouri Botanical Garden CY OCT 08-10, 2004 CL St Louis, MO DE climate; human land use; prehistoric agriculture Quaternary history; seasonal tropical forests; slash and burn cultivation; vegetation ID LAST GLACIAL MAXIMUM; LOW ATMOSPHERIC CO2; CLIMATE-CHANGE; POLLEN RECORD; RAIN-FOREST; PHYTOLITH ANALYSIS; MAIZE CULTIVATION; HUMAN DISTURBANCE; LOWLAND AMAZONIA; HUMAN OCCUPATION AB The corpus of historical data from lake sediments relating to the climate, vegetation, and human land use of the lowland Central American tropical forest between ca. 20,000 BP and the time of European contact is reviewed. Pollen, phytolith, and charcoal records identify the distribution and composition of tropical vegetation and fire patterns during the late Pleistocene, when they were significantly altered from today's, and earliest Holocene, when plant communities reassembled and interglacial representatives began to coalesce on the landscape. The significance of the environmental perturbations that occurred during the transition from the Pleistocene to the Holocene for human occupation of the lowland tropical forest and the geography and chronology of agricultural origins is discussed. Fire was employed by hunters and gatherers and farmers alike during the past 11,000 years as a primary tool of forest modification. The profound effects of an ancient pre-Columbian development of plant food production and, subsequently, slash and burn agriculture between ca. 10,000 BP and 4000 BP can be seen on lowland forests from Mexico to the Amazon Basin. C1 Smithsonian Trop Res Inst, Panama City, Panama. Museum Natl Hist Nat, Dept Anthropol, Washington, DC USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM pipernod@si.edu NR 117 TC 37 Z9 38 U1 2 U2 22 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2006 VL 93 IS 2 BP 274 EP 296 DI 10.3417/0026-6493(2006)93[274:QEHAAI]2.0.CO;2 PG 23 WC Plant Sciences SC Plant Sciences GA 077ZV UT WOS:000240071400007 ER PT S AU Gaensler, BM Slane, PO AF Gaensler, Bryan M. Slane, Patrick O. TI The evolution and structure of pulsar wind nebulae SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE acceleration of particles; magnetic fields; shock waves; supernova remnants; winds and outflows ID SUPERNOVA REMNANT G21.5-0.9; BOW-SHOCK NEBULAE; RELATIVISTIC MHD SIMULATIONS; EXACT ANALYTIC SOLUTIONS; HUBBLE-SPACE-TELESCOPE; SOFT GAMMA-REPEATERS; HIGH-ENERGY EMISSION; X-RAY-EMISSION; CRAB-NEBULA; NEUTRON-STAR AB Pulsars steadily dissipate their rotational energy via relativistic winds. Confinement of these outflows generates luminous pulsar wind nebulae, seen across the electromagnetic spectrum in synchrotron and inverse Compton emission and in optical emission lines when they shock the surrounding medium. These sources act as import-ant probes of relativistic shocks, particle acceleration, and interstellar gas. We review the many recent advances in the study of pulsar wind nebulae, with particular focus on the evolutionary stages through which these objects progress as they expand into their surroundings, and on morphological structures within these nebulae that directly trace the physical processes of particle acceleration and outflow. We conclude by considering some exciting new probes of pulsar wind nebulae, including the study of TeV gamma-ray emission from these sources, and observations of pulsar winds in close binary systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu; pslane@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 153 TC 319 Z9 321 U1 2 U2 10 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 BN 978-0-8243-0944-2 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 17 EP 47 DI 10.1146/annurev.astro.44.051905.092528 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100003 ER PT S AU Remillard, RA McClintock, JE AF Remillard, Ronald A. McClintock, Jeffrey E. TI X-ray properties of black-hole binaries SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE accretion physics; black holes; general relativity; X-ray sources ID QUASI-PERIODIC OSCILLATIONS; MICROQUASAR GRO J1655-40; RXTE SPECTRAL OBSERVATIONS; CANDIDATE XTE J1550-564; DISC INSTABILITY MODEL; ALPHA EMISSION-LINE; HIGH-FREQUENCY QPOS; XMM-NEWTON/EPIC-PN; ACCRETION DISK; HIGH-STATE AB We review the properties and behavior of 20 X-ray binaries that contain a dynamically-confirmed black hole, 17 of which are transient systems. During the past decade, many of these transient sources were observed daily throughout the course of their typically year-long outburst cycles using the large-area timing detector aboard the Rossi X-Ray Timing Explorer. The evolution of these transient sources is complex. Nevertheless, there are behavior patterns common to all of them as we show in a comprehensive comparison of six selected systems. Central to this comparison are three X-ray states of accretion, which are reviewed and defined quantitatively. We discuss phenomena that arise in strong gravitational fields, including relativistically-broadened Fe lines, high-frequency quasi-periodic oscillations (100-450 Hz), and relativistic radio and X-ray jets. Such phenomena show us how a black hole interacts with its environment, thereby complementing the picture of black holes that gravitational wave detectors will provide. We sketch a scenario for the potential impact of timing/spectral studies of accreting black holes on physics and discuss a current frontier topic, namely, the measurement of black hole spin. C1 MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Remillard, RA (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rr@space.init.edu; jem@cfa.harvard.edu NR 180 TC 913 Z9 918 U1 4 U2 37 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 BN 978-0-8243-0944-2 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 49 EP 92 DI 10.1146/annurev.astro.44.051905.092532 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100004 ER PT S AU Werner, M Fazio, G Rieke, G Roellig, TL Watson, DM AF Werner, Michael Fazio, Giovanni Rieke, George Roellig, Thomas L. Watson, Dan M. TI First fruits of the Spitzer Space Telescope: Galactic and solar system studies SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE brown dwarfs; circumstellar disks; exoplanets; infrared astronomy; planetary system formation; space technology; star formation; stellar evolution ID LARGE-MAGELLANIC-CLOUD; YOUNG STELLAR OBJECTS; SUPERNOVA REMNANT CASSIOPEIA; MAIN-SEQUENCE STARS; T-TAURI STARS; TERRESTRIAL PLANET FORMATION; VEGA-LIKE STARS; KUIPER-BELT; BETA-PICTORIS; DEBRIS DISKS AB The Spitzer Space Telescope, launched in August 2003, is the infrared member of NASAs Great Observatory family. Spitzer combines the intrinsic sensitivity of a cryogenic telescope in space with the imaging and spectroscopic power of modern infrared detector arrays. This review covers early results from Spitzer that have produced major advances in our understanding of our own solar system and phenomena within the Galaxy. Spitzer has made the first detection of light from extrasolar planets, characterized planet-forming and planetary debris disks around solar-type stars, showed that substellar objects with masses smaller than 10 M(Jup) form through the same processes as do solar-mass stars, and studied in detail the composition of cometary ejecta in our Solar System. Spitzer major technical advances will pave the way for yet more powerful future instruments. Spitzer should operate with full capabilities well into 2009, enabling several additional cycles of discovery and follow-up. C1 CALTECH, Jet Prop Lab, Astron & Phys Directorate, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Werner, M (reprint author), CALTECH, Jet Prop Lab, Astron & Phys Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mwerner@sirtfweb.jpl.nasa.gov; gfazio@cfa.harvard.edu; grieke@as.arizona.edu; thomas.l.roellig@nasa.gov; dmw@pas.rochester.edu NR 193 TC 33 Z9 33 U1 0 U2 3 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 BN 978-0-8243-0944-2 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 269 EP 321 DI 10.1146/annurev.astro.44.051905.092544 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100008 ER PT S AU Fabbiano, G AF Fabbiano, G. TI Populations of X-ray sources in galaxies SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE galaxies; globular clusters; stellar populations; supersoft X-ray sources; ultraluminous X-ray sources (ULXs); X-ray binaries; X-ray sources ID MASS BLACK-HOLES; XMM-NEWTON OBSERVATIONS; HIGH-RESOLUTION CAMERA; STAR-FORMING GALAXIES; MULTIVARIATE STATISTICAL-ANALYSIS; GLOBULAR CLUSTER CONNECTION; FORMATION RATE INDICATOR; POINT-SOURCE POPULATION; ROSAT PSPC OBSERVATIONS; DWARF STARBURST GALAXY AB Today's sensitive X-ray observations allow the study of populations of X-ray binaries in galaxies as distant as 20-30 Mpc. Photometric diagrams and luminosity functions applied to these populations provide a direct probe of the evolved binary component of different stellar populations. The study of the X-ray populations of E and SO galaxies has revamped the debate on the formation and evolution of low-mass X-ray binaries (LMXBs) and on the role of globular clusters in these processes. Though overall stellar mass drives the amount of X-ray binaries in old stellar populations, the amount of sources in star-forming galaxies is related to the star-formation rate. Short-lived, luminous, high-mass X-ray binaries (HMXBs) dominate these young X-ray populations. The most luminous sources in these systems are the debated ultraluminous X-ray sources (ULXs). Observations of the deep X-ray sky, and comparison with deep optical surveys, are providing the first evidence of the X-ray evolution of galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu NR 270 TC 190 Z9 190 U1 2 U2 8 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 BN 978-0-8243-0944-2 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 323 EP 366 DI 10.1146/annurev.astro.44.051905.092519 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100009 ER PT J AU Harris, DE Krawczynski, H AF Harris, D. E. Krawczynski, Henric TI X-ray emission from extragalactic jets SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE inverse Compton ernission; relativistic jets; synchrotron emission; X-ray jets ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; LARGE-SCALE JETS; DOUBLE RADIO-SOURCES; ELECTRON-POSITRON JETS; CHANDRA OBSERVATIONS; PARTICLE-ACCELERATION; M87 JET; RELATIVISTIC JETS; GALAXY 3C-31 AB This review focuses on the X-ray emission processes of extragalactic jets on scales resolvable by the subarcsec resolution of the Chandra X-ray Observatory. It is divided into four parts. The introductory section reviews the classical problems for jets, as well as those associated directly with the X-ray emission. Throughout this section, we deal with the dualisms of low-powered radio sources versus high-powered radio galaxies and quasars and of synchrotron models versus inverse Compton models; and the distinction between the relativistic plasma responsible for the received radiation and the medium responsible for the transport of energy down the jet. The second section collects the observational and inferred parameters for the currently detected X-ray jets and attempts to put their relative sizes and luminosities in perspective. In the third section we first give the relevant radio and optical jet characteristics, and then examine the details of the X-ray data and how they can be related to various jet attributes. The last section is devoted to a critique of the two nonthermal emission processes and to prospects for progress in our understanding of jets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Washington Univ, St Louis, MO 63130 USA. RP Harris, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM harris@cfa.harvard.edu; krawcz@wuphys.wustl.edu NR 149 TC 119 Z9 120 U1 1 U2 6 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 463 EP 506 DI 10.1146/annurev.astro.44.051905.092446 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100012 ER PT J AU Bambach, RK AF Bambach, Richard K. TI Phanerozoic biodiversity mass extinctions SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES SE Annual Review of Earth and Planetary Sciences LA English DT Review; Book Chapter DE paleobiology; evolution; macroevolution; selectivity of extinction; timing of extinction ID PERMIAN-TRIASSIC BOUNDARY; CARBON-ISOTOPE STRATIGRAPHY; OCEANIC ANOXIC EVENT; SEA-LEVEL CHANGE; FOSSIL RECORD; SOUTH CHINA; BIOTIC CRISIS; MARINE REALM; DEEP-WATER; END AB Recent analyses of Sepkoski's genus-level compendium show that only three events form a statistically separate class of high extinction intensities when only post-Early Ordovician intervals are considered, but geologists have called numerous events mass extinctions. Is this a conflict? A review of different methods of tabulating data from the Sepkoski database reveals 18 intervals during the Phanerozoic have peaks of both magnitude and rate of extinction that appear in each tabulating scheme. These intervals all fit Sepkoski's definition of mass extinction. However, they vary widely in timing and effect of extinction, demonstrating that mass extinctions are not a homogeneous group of events. No consensus has been reached on the kill mechanism for any marine mass extinction. In fact, adequate data on timing in ecologic, rather than geologic, time and on geographic and environmental distribution of extinction have not yet been systematically compiled for any extinction event. C1 Harvard Herbaria, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Museum Nat Hist, Cambridge, MA 02138 USA. Virginia Tech, Blacksburg, VA 24061 USA. RP Bambach, RK (reprint author), Harvard Herbaria, Cambridge, MA 02138 USA. EM richard.bambach@verizon.net NR 124 TC 135 Z9 140 U1 6 U2 68 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2006 VL 34 BP 127 EP 155 DI 10.1146/annurev.earth.33.092203.122654 PG 29 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 054MI UT WOS:000238380600006 ER PT S AU Willis, BL van Oppen, MJH Miller, DJ Vollmer, SV Ayre, DJ AF Willis, Bette L. van Oppen, Madeleine J. H. Miller, David J. Vollmer, Steve V. Ayre, David J. TI The role of hybridization in the evolution of reef corals SO ANNUAL REVIEW OF ECOLOGY EVOLUTION AND SYSTEMATICS SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE acropora; hybridfitness; introgression; reticulate evolution; sperm choice crosses ID MONTASTRAEA-ANNULARIS COMPLEX; SPECIES GROUP CNIDARIA; REPRODUCTIVE ISOLATION; GENUS ACROPORA; HYBRID ZONES; SCLERACTINIAN CORALS; MITOCHONDRIAL-DNA; GENETIC-EVIDENCE; SPAWNING CORALS; CLIMATE-CHANGE AB The importance of hybridization in the evolution of plant species is widely accepted, but its contributions to animal species evolution remain less recognized. Here we review evidence that hybridization has contributed to the evolution of reef corals, a group underpinning the coral reef ecosystem. Increasingly threatened by human and climate-related impacts, there is need to understand the evolutionary processes that have given rise to their diversity and contribute to their resilience. Reticulate evolutionary pathways among the ecologically prominent, mass-spawning genus Acropora suggest that hybridization, although rare on ecological timescales, has been instrumental in their diversification on evolutionary timescales. Evidence that coral hybrids colonize marginal habitats distinct from those of parental species' and that hybridization may be more frequent at peripheral boundaries of species' ranges supports a role for hybridization in range expansion and adaptation to changing environments. We conclude that outcomes of hybridization are significant for the future resilience of reef corals and warrant inclusion in conservation strategies. C1 James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. Australian Inst Marine Sci, Townsville, Qld 4810, Australia. James Cook Univ N Queensland, Comparat Genom Ctr, Townsville, Qld 4811, Australia. Smithsonian Trop Res Inst, Balboa, Panama. Univ Wollongong, Sch Biol Sci, Wollongong, NSW 2522, Australia. RP Willis, BL (reprint author), James Cook Univ N Queensland, Sch Marine Biol & Aquaculture, Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. EM Bette.willis@jcu.edu.au; m.vanoppen@aims.gov.au; David.Miller@jcu.edu.au; vollmers@si.edu; dja@uow.edu.au RI Ayre, David/A-8761-2008; van Oppen, Madeleine/C-3261-2008; OI Ayre, David/0000-0002-3124-4417; van Oppen, Madeleine/0000-0003-4607-0744 NR 106 TC 100 Z9 110 U1 3 U2 42 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1543-592X BN 978-0-8243-1437-8 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2006 VL 37 BP 489 EP 517 DI 10.1146/annurev.ecolsys.37.091305.110136 PG 29 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 119UE UT WOS:000243038500018 ER PT J AU Honeychurch, W Amartuvshin, C AF Honeychurch, William Amartuvshin, Chunag BE Stark, MT TI States on Horseback: The Rise of Inner Asian Confederations and Empires SO ARCHAEOLOGY OF ASIA SE Blackwell Studies in Global Archaeology LA English DT Article; Book Chapter ID PERSPECTIVES C1 [Honeychurch, William] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Amartuvshin, Chunag] Inst Archaeol, Ulaanbaatar, Mongol Peo Rep. RP Honeychurch, W (reprint author), Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 39 TC 28 Z9 28 U1 0 U2 4 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-0-47077-467-0 J9 BLACKW STUD GLOB ARC PY 2006 BP 255 EP 278 DI 10.1002/9780470774670.ch12 D2 10.1002/9780470774670 PG 24 WC Archaeology SC Archaeology GA BYG02 UT WOS:000298538500013 ER PT J AU Kirwin, L AF Kirwin, Liza TI Art and space: Park Place and the beginning of the Paula Cooper Gallery SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kirwin, L (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2006 VL 46 IS 1-2 BP 36 EP 40 PG 5 WC Art SC Art GA 145RV UT WOS:000244883100004 ER PT J AU Ward, DC AF Ward, David C. TI Looking into Walt Whitman: American art, 1850-1920. SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Ward, DC (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2006 VL 46 IS 1-2 BP 41 EP 45 PG 5 WC Art SC Art GA 145RV UT WOS:000244883100005 ER PT S AU McCarthy, MC AF McCarthy, Michael C. BE Kaiser, RI Bernath, P Osamura, Y Petrie, S Mebel, AM TI Laboratory astrophysics and radio astronomy: Some recent successes SO Astrochemistry: From Laboratory Studies to Astronomical Observations SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Astrochemistry - From Laboratory Studies to Astronomical Observations CY DEC 18-20, 2005 CL Honolulu, HI SP Amer Chem Soc, Natl Sci Fdn DE rotational spectroscopy; radio astronomy; ISM : molecules; molecular data ID ROTATIONAL SPECTRUM; HYPERFINE-STRUCTURE; MICROWAVE-SPECTRUM; CH; IRC+10216; DISCHARGE; MOLECULES; STATE; SINC; SICN AB This paper presents several examples illustrating how the close coordination of laboratory astrophysics and radio astronomy can lead to an improved understanding of the rich chemistry of circumstellar shells which surround evolved carbon stars and dense molecular clouds. State-of-the-art microwave techniques in combination with supersonic molecular beam techniques and long path absorption spectroscopy at millimeter-wave wavelengths are used here to determine precise rest frequencies of known or postulated reactive molecules of astrophysical interest. Because the astronomically most interesting lines either have been measured or can be calculated to better than 1 km/sec in equivalent radial velocity, dedicated astronomical searches can be undertaken with confidence, and the carriers of unidentified series of astronomical lines can be established with certainty. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0351-1 J9 AIP CONF PROC PY 2006 VL 855 BP 209 EP 218 PG 10 WC Astronomy & Astrophysics; Chemistry, Analytical SC Astronomy & Astrophysics; Chemistry GA BFD89 UT WOS:000241319800025 ER PT J AU Grupe, D Mathur, S Wilkes, B Osmer, P AF Grupe, D Mathur, S Wilkes, B Osmer, P TI XMM-Newton observations of high-redshift quasars SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : active; quasars : general; quasars : individual (BR 2237-0607, BR 0351-1034) ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SOFT-X-RAY; BLACK-HOLE MASS; EXPLORATORY CHANDRA OBSERVATIONS; MULTIWAVELENGTH PROJECT CHAMP; BAND ENERGY-DISTRIBUTION; LINE SEYFERT-1 GALAXIES; ROSAT DETECTED QUASARS; RADIO-SELECTED QUASAR AB We report on our XMM-Newton observations of the high-redshift quasars BR 2237-0607 (z = 558) and BR 0351-1034 (z = 351). We also report on XMM-Newton observations of 19 other z > 4 objects available in the public archive of which 14 were detected. We find that the optical to X-ray spectral index alpha(ox) is correlated with the luminosity density at 2500 angstrom but does not show a correlation with redshift, which is consistent with earlier results. Radio-loud quasars are brighter and have flatter X-ray slopes compared to radio-quiet quasars. There is some evidence for the jet-dominated sources to be intrinsically absorbed. The mean intrinsic 2-10 keV power-law slope of the 10 high-redshift radio-quiet quasars in our sample for which a spectral analysis can be performed is alpha(X) = 1.21 +/- 0.52 (ranging between 0.32 and 1.96), which is more like the alpha(X) = 1.19 +/- 0: 10 found from the ASCA observations of low-redshift narrow-line Seyfert 1 galaxies (NLS1s) but different from the alpha(X) = 0.78 +/- 0.11 found for low-redshift broad-line Seyfert galaxies. The steep X-ray spectral index suggests high Eddington ratios L/L-Edd. These observations give credence to the hypothesis of Mathur that NLS1s are low-luminosity cousins of high-redshift quasars. Comparison with other results from the literature indicates that perhaps the most luminous quasars, from low to high redshift, have similarly steep X-ray spectra suggestive of high Eddington luminosities. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM dgrupe@astronomy.ohio-state.edu; smita@astronomy.ohio-state.edu; belinda@head.cfa.harvard.edu; posmer@astronomy.ohio-state.edu OI Wilkes, Belinda/0000-0003-1809-2364 NR 112 TC 22 Z9 22 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JAN PY 2006 VL 131 IS 1 BP 55 EP 69 DI 10.1086/498260 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300006 ER PT J AU Covey, KR Greene, TP Doppmann, GW Lada, CJ AF Covey, KR Greene, TP Doppmann, GW Lada, CJ TI The radial velocity distribution of class I and flat-spectrum protostars SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; stars : kinematics; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID T-TAURI STARS; MOLECULAR CLOUDS; BROWN DWARFS; MILKY-WAY; AURIGA; MULTIPLICITY; SPECTROSCOPY; ACCRETION; CLUSTERS; SYSTEMS AB We analyze radial velocities for a sample of 31 Class I and flat-spectrum protostars in Taurus-Auriga, rho Ophiuchi, and Serpens for evidence of the global dynamical state of extremely young stellar populations buried within parental molecular clouds. Comparing the radial velocity of each protostar to that of the local CO gas, we are able to constrain the one-dimensional radial velocity dispersion of Class I and flat-spectrum objects to similar to 2.5 km s(-1) or below. This upper limit to the protostellar velocity dispersion is consistent with the velocity dispersions of surrounding CO gas, which we measure to be similar to 1.4 km s(-1), suggesting that the motions of protostars and local CO gas are dynamically linked and are dominated by the gravitational potential of the molecular cloud. However, the upper limit on the protostellar velocity dispersion could still allow for slightly inflated motions of protostars relative to the local molecular gas. Four of the protostars analyzed appear to have velocities more than 3 sigma (7.5 km s(-1)) away from the central local CO gas velocity while showing spectroscopic indicators of youth and accretion such as H-2 emission, H I Br gamma emission, or K-band continuum veiling. These radial velocity outliers may represent protostellar spectroscopic binaries or ejected cluster members. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Covey, KR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. OI Covey, Kevin/0000-0001-6914-7797 NR 38 TC 27 Z9 27 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 JAN PY 2006 VL 131 IS 1 BP 512 EP 519 DI 10.1086/498064 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300037 ER PT J AU Jha, S Kirshner, RP Challis, P Garnavich, PM Matheson, T Soderberg, AM Graves, GJM Hicken, M Alves, JF Arce, HG Balog, Z Barmby, P Barton, EJ Berlind, P Bragg, AE Briceno, C Brown, WR Buckley, JH Caldwell, N Calkins, ML Carter, BJ Concannon, KD Donnelly, RH Eriksen, KA Fabricant, DG Falco, EE Fiore, F Garcia, MR Gomez, M Grogin, NA Groner, T Groot, PJ Haisch, KE Hartmann, L Hergenrother, CW Holman, MJ Huchra, JP Jayawardhana, R Jerius, D Kannappan, SJ Kim, DW Kleyna, JT Kochanek, CS Koranyi, DM Krockenberger, M Lada, CJ Luhman, KL Luu, JX Macri, LM Mader, JA Mahdavi, A Marengo, M Marsden, BG McLeod, BA McNamara, BR Megeath, ST Moraru, D Mossman, AE Muench, AA Munoz, JA Muzerolle, J Naranjo, O Nelson-Patel, K Pahre, MA Patten, BM Peters, J Peters, W Raymond, JC Rines, K Schild, RE Sobczak, GJ Spahr, TB Stauffer, JR Stefanik, RP Szentgyorgyi, AH Tollestrup, EV Vaisanen, P Vikhlinin, A Wang, Z Willner, SP Wolk, SJ Zajac, JM Zhao, P Stanek, KZ AF Jha, S Kirshner, RP Challis, P Garnavich, PM Matheson, T Soderberg, AM Graves, GJM Hicken, M Alves, JF Arce, HG Balog, Z Barmby, P Barton, EJ Berlind, P Bragg, AE Briceno, C Brown, WR Buckley, JH Caldwell, N Calkins, ML Carter, BJ Concannon, KD Donnelly, RH Eriksen, KA Fabricant, DG Falco, EE Fiore, F Garcia, MR Gomez, M Grogin, NA Groner, T Groot, PJ Haisch, KE Hartmann, L Hergenrother, CW Holman, MJ Huchra, JP Jayawardhana, R Jerius, D Kannappan, SJ Kim, DW Kleyna, JT Kochanek, CS Koranyi, DM Krockenberger, M Lada, CJ Luhman, KL Luu, JX Macri, LM Mader, JA Mahdavi, A Marengo, M Marsden, BG McLeod, BA McNamara, BR Megeath, ST Moraru, D Mossman, AE Muench, AA Munoz, JA Muzerolle, J Naranjo, O Nelson-Patel, K Pahre, MA Patten, BM Peters, J Peters, W Raymond, JC Rines, K Schild, RE Sobczak, GJ Spahr, TB Stauffer, JR Stefanik, RP Szentgyorgyi, AH Tollestrup, EV Vaisanen, P Vikhlinin, A Wang, Z Willner, SP Wolk, SJ Zajac, JM Zhao, P Stanek, KZ TI UBVRI light curves of 44 type Ia supernovae SO ASTRONOMICAL JOURNAL LA English DT Article DE supernovae : general; techniques : photometric ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; INFRARED PHOTOMETRY; CONSTANT; CONSTRAINTS; EXTINCTION; LUMINOSITY; LAMBDA; DECELERATION AB We present UBVRI photometry of 44 Type Ia supernovae (SNe Ia) observed from 1997 to 2001 as part of a continuing monitoring campaign at the Fred Lawrence Whipple Observatory of the Harvard-Smithsonian Center for Astrophysics. The data set comprises 2190 observations and is the largest homogeneously observed and reduced sample of SNe Ia to date, nearly doubling the number of well-observed, nearby SNe Ia with published multicolor CCD light curves. The large sample of U-band photometry is a unique addition, with important connections to SNe Ia observed at high redshift. The decline rate of SN Ia U-band light curves correlates well with the decline rate in other bands, as does the U-B color at maximum light. However, the U-band peak magnitudes show an increased dispersion relative to other bands even after accounting for extinction and decline rate, amounting to an additional similar to 40% intrinsic scatter compared to the B band. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jha, S (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA. EM saurabh@astron.berkeley.edu RI Barmby, Pauline/I-7194-2016; Groot, Paul/K-4391-2016; OI Barmby, Pauline/0000-0003-2767-0090; Groot, Paul/0000-0002-4488-726X; Wolk, Scott/0000-0002-0826-9261; Alves, Joao/0000-0002-4355-0921; Fiore, Fabrizio/0000-0002-4031-4157; Macri, Lucas/0000-0002-1775-4859 NR 62 TC 192 Z9 192 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 JAN PY 2006 VL 131 IS 1 BP 527 EP 554 DI 10.1086/497989 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300039 ER PT J AU Harris, HC Munn, JA Kilic, M Liebert, J Williams, KA von Hippel, T Levine, SE Monet, DG Eisenstein, DJ Kleinman, SJ Metcalfe, TS Nitta, A Winget, DE Brinkmann, J Fukugita, M Knapp, GR Lupton, RH Smith, JA Schneider, DP AF Harris, HC Munn, JA Kilic, M Liebert, J Williams, KA von Hippel, T Levine, SE Monet, DG Eisenstein, DJ Kleinman, SJ Metcalfe, TS Nitta, A Winget, DE Brinkmann, J Fukugita, M Knapp, GR Lupton, RH Smith, JA Schneider, DP TI The white dwarf luminosity function from Sloan Digital Sky Survey imaging data SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; solar neighborhood; stars : kinematics; stars : luminosity function, mass function white; dwarfs ID PROPER MOTION STARS; MONTE-CARLO SIMULATIONS; CETI INSTABILITY STRIP; HALO DARK-MATTER; DATA RELEASE; USNO-B; TRIGONOMETRIC PARALLAX; NORTHERN STARS; GALACTIC DISK; HYDROGEN-RICH AB A sample of white dwarfs is selected from the Sloan Digital Sky Survey (SDSS) Data Release 3 using their reduced proper motions, based on improved proper motions from combined SDSS and USNO-B data. Numerous SDSS and follow-up spectra (Kilic and coworkers) are used to quantify completeness and contamination of the sample; kinematics models are used to understand and correct for velocity-dependent selection biases. A luminosity function is constructed covering the range 7 < M-bol < 16, and its sensitivity to various assumptions and selection limits is discussed. The white dwarf luminosity function based on 6000 stars is remarkably smooth and rises nearly monotonically to M-bol = 15.3. It then drops abruptly, although the small number of low-luminosity stars in the sample and their unknown atmospheric composition prevent quantitative conclusions about this decline. Stars are identified that may have high tangential velocities, and a preliminary luminosity function is constructed for them. C1 USN Observ, Flagstaff, AZ 86001 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Apache Point Obser, Sunspot, NM 88349 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. Princeton Univ Observ, Princeton, NJ 08544 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Harris, HC (reprint author), USN Observ, 10391 W Naval Observ Rd, Flagstaff, AZ 86001 USA. EM hch@nofs.navy.mil RI Metcalfe, Travis/A-9388-2008; OI Metcalfe, Travis/0000-0003-4034-0416; Williams, Kurtis/0000-0002-1413-7679 NR 68 TC 120 Z9 120 U1 1 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 JAN PY 2006 VL 131 IS 1 BP 571 EP 581 DI 10.1086/497966 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300042 ER PT J AU Kilic, M Munn, JA Harris, HC Liebert, J von Hippel, T Williams, KA Metcalfe, TS Winget, DE Levine, SE AF Kilic, M Munn, JA Harris, HC Liebert, J von Hippel, T Williams, KA Metcalfe, TS Winget, DE Levine, SE TI Cool white dwarfs in the Sloan Digital Sky Survey SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : atmospheres; stars : evolution; white dwarfs ID 1ST DATA RELEASE; LUMINOSITY FUNCTION; GALACTIC DISK; DARK-MATTER; USNO-B; STARS; CATALOG; AGE; OLD AB A reduced proper motion diagram utilizing Sloan Digital Sky Survey (SDSS) photometry and astrometry and USNO-B plate astrometry is used to separate cool white dwarf candidates from metal-weak, high-velocity, main-sequence Population II stars (subdwarfs) in the SDSS Data Release 2 imaging area. Follow-up spectroscopy using the Hobby-Eberly Telescope, the MMT, and the McDonald 2.7 m telescope is used to demonstrate that the white dwarf and subdwarf loci separate cleanly in the reduced proper motion diagram and that the contamination by subdwarfs is small near the cool white dwarf locus. This enables large, statistically complete samples of white dwarfs, particularly the poorly understood cool white dwarfs, to be created from the SDSS imaging survey, with important implications for white dwarf luminosity function studies. SDSS photometry for our sample of cool white dwarfs is compared to current white dwarf models. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. USN Observ, Flagstaff, AZ 86001 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kilic, M (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM kilic@astro.as.utexas.edu RI Metcalfe, Travis/A-9388-2008; OI Metcalfe, Travis/0000-0003-4034-0416; Williams, Kurtis/0000-0002-1413-7679 NR 48 TC 73 Z9 73 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 JAN PY 2006 VL 131 IS 1 BP 582 EP 599 DI 10.1086/497962 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300043 ER PT J AU Schuster, MT Humphreys, RM Marengo, M AF Schuster, MT Humphreys, RM Marengo, M TI The circumstellar environments of NML CYGNI and the cool hypergiants SO ASTRONOMICAL JOURNAL LA English DT Article DE stars : individual ( p cassiopeiae, NML Cygni, S Persei, VX Sagittarii); supergiants ID VY-CANIS-MAJORIS; RHO-CASSIOPEIAE; MASSIVE STARS; MILKY-WAY; MERLIN OBSERVATIONS; YELLOW HYPERGIANTS; NEARBY GALAXIES; HIGH-RESOLUTION; LUMINOUS STARS; VX SAGITTARIUS AB We present high-resolution HST WFPC2 images of compact nebulosity surrounding the cool M-type hypergiants NML Cyg, VX Sgr, and S Per. The powerful OH/IR source NML Cyg exhibits a peculiar bean-shaped asymmetric nebula that is coincident with the distribution of its H2O vapor masers. We show that NML Cyg's circumstellar envelope is likely shaped by photodissociation from the powerful, nearby association Cyg OB2 inside the Cygnus X superbubble. The OH/IR sources VX Sgr and S Per have marginally resolved envelopes. S Per's circumstellar nebula appears elongated in a northeast/southwest orientation similar to that for its OH and H2O masers, while VX Sgr is embedded in a spheroidal envelope. We find no evidence for circumstellar nebulosity around the intermediate-type hypergiants rho Cas, HR 8752, and HR 5171a, nor around the normal M-type supergiant mu Cep. We conclude that there is no evidence for high mass loss events prior to 500-1000 years ago for these four stars. C1 Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schuster, MT (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. EM mschuster@cfa.harvard.edu; roberta@aps.umn.edu; mmarengo@cfa.harvard.edu NR 54 TC 35 Z9 35 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 JAN PY 2006 VL 131 IS 1 BP 603 EP 611 DI 10.1086/498395 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300045 ER PT J AU Gaensier, BM AF Gaensier, B. M. TI The Square Kilometre Array: a new probe of cosmic magnetism SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT International Conference on Origin and Evolution of Cosmic Magnetism CY AUG 29-SEP 02, 2005 CL Bologna, ITALY SP Ist Radioastron INAF DE cosmology : large-scale structure; Galaxy : structure; intergalactic medium; magnetic fields; instrumentation : interferometers; techniques : polarimetric ID FARADAY-ROTATION SEARCH; INTERGALACTIC SHOCKS; RADIO-CONTINUUM; FIELDS; GALAXIES; EVOLUTION; CLUSTER; SKY; DEPOLARIZATION; EMISSION AB Magnetic fields are a fundamental part of many astrophysical phenomena, but the evolution, structure and origin of magnetic fields are still unresolved problems in physics and astrophysics. When and how were the first fields generated? Are present-day magnetic fields the result of standard dynamo action, or do they represent rapid or recent field amplification through other processes? What role do magnetic fields play in turbulence, cosmic ray acceleration and structure formation? I explain how the Square Kilometre Array (SKA), a next-generation radio telescope, can deliver stunning new data-sets that will address these currently unanswered issues. The foundation for these experiments will be an all-sky survey of rotation measures, in which Faraday rotation toward > 10(7) background sources will provide a dense grid for probing magnetism in the Milky Way, nearby galaxies, and in distant galaxies, clusters and protogalaxies. Using these data, we can map out the evolution of magnetized structures from redshifts z > 3 to the present, can distinguish between different origins for seed magnetic fields in galaxies, and can develop a detailed model of the magnetic field geometry of the intergalactic medium and of the overall Universe. In addition, the SKA will certainly discover new magnetic phenomena beyond what we can currently predict or imagine. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaensier, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu OI Gaensler, Bryan/0000-0002-3382-9558 NR 58 TC 10 Z9 10 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 5-6 BP 387 EP 394 DI 10.1002/asna.200610539 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063WD UT WOS:000239049700002 ER PT J AU Haverkorn, M Gaensler, BM Brown, JAC McClure-Griffiths, NM Dickey, JM Green, AJ AF Haverkorn, M. Gaensler, B. M. Brown, J. -A. C. McClure-Griffiths, N. M. Dickey, J. M. Green, A. J. TI Magnetic fields in the Southern Galactic Plane Survey SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT International Conference on Origin and Evolution of Cosmic Magnetism CY AUG 29-SEP 02, 2005 CL Bologna, ITALY SP Ist Radioastron INAF DE ISM : magnetic fields; ISM : structure; surveys; radio continuum : ISM; turbulence ID SPIRAL STRUCTURE; INNER GALAXY; EMISSION; TURBULENCE AB The Southern Galactic Plane Survey (SGPS) is a 1.4 GHz radio polarization and H I survey in a large part of the inner Galactic plane at a resolution of about an arcmin. Depolarization and Faraday rotation of polarized radiation from diffuse Galactic synchrotron emission, pulsars, and extragalactic sources can be used to infer information about the strength and structure of the Galactic magnetic field. Here, we discuss early results of the polarization data from the SGPS. We show from statistical analysis of rotation measures of polarized extragalactic sources that fluctuations in the magnetoionized medium of the spiral arms are probably mainly caused by H II regions, while the rotation measure fluctuations in the interarm regions may be connected to the interstellar turbulent cascade. Furthermore, the variations of rotation measure with Galactic longitude enable modeling of the large-scale component of the Galactic magnetic field, including determination of the number and location of magnetic field reversals. Finally, the SGPS is an excellent way to study subparsec-scale structure in the ionized interstellar medium by way of depolarization studies in H II regions. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Haverkorn, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94704 USA. EM mhaverkorn@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; Dickey, John/C-6156-2013; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Dickey, John/0000-0002-6300-7459; Gaensler, Bryan/0000-0002-3382-9558 NR 21 TC 2 Z9 2 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 5-6 BP 483 EP 486 DI 10.1002/asna.200610565 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063WD UT WOS:000239049700028 ER PT J AU Giacintucci, S Mazzotta, P Brunetti, G Venturi, T Bardelli, S AF Giacintucci, S. Mazzotta, P. Brunetti, G. Venturi, T. Bardelli, S. TI Evidence of gas heating by the central AGN in MKW 3s SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT International Conference on Origin and Evolution of Cosmic Magnetism CY AUG 29-SEP 02, 2005 CL Bologna, ITALY SP Ist Radioastron INAF DE galaxies : clusters : individual (MKW 3s); cooling flows; radio continuum : galaxies; X-rays : galaxies : clusters ID COOLING FLOWS; CLUSTERS AB We present the results of radio observations of the galaxy cluster MKW 3s carried out at 1.28 GHz and 610 MHz with the Giant Metrewave Radio Telescope (GMRT). The Chandra observations of MKW 3s revealed that this cluster is characterized by a complex X-ray structure hosting both a X-ray filament and a X-ray cavity. The temperature structure of the cluster core is even more complex, with the presence of extended regions of gas heated above the radially averaged gas temperature at any radius. The magnetic field derived from the radio observations is similar to 2 mu G and provides radiative ages of the order of similar to 2 x 10(8) yrs. Thanks to this estimate of the magnetic field strength and the comparison between the radio structure and the Chandra data, we found clear evidence for a close connection between the radio activity of the central AGN and the heated gas regions in this cluster. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy. IRA, INAF, Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. EM sgiaci.s@ira.ira.inaf.it RI Bardelli, Sandro/O-9369-2015; Mazzotta, Pasquale/B-1225-2016; OI Bardelli, Sandro/0000-0002-8900-0298; Mazzotta, Pasquale/0000-0002-5411-1748; Venturi, Tiziana/0000-0002-8476-6307; Brunetti, Gianfranco/0000-0003-4195-8613 NR 5 TC 2 Z9 2 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 5-6 BP 573 EP 574 DI 10.1002/asna.200610594 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063WD UT WOS:000239049700057 ER PT J AU Allan, A Hessman, F Bischoff, K Burgdorf, M Cavanagh, B Christian, D Clay, N Dickens, R Economou, F Fadavi, M Fraser, S Granzer, T Grosvenor, S Jenness, T Koratkar, A Lehner, M Mottram, C Naylor, T Saunders, E Solomos, N Steele, I Tuparev, G Vestrand, T White, R Yost, S AF Allan, A. Hessman, F. Bischoff, K. Burgdorf, M. Cavanagh, B. Christian, D. Clay, N. Dickens, R. Economou, F. Fadavi, M. Fraser, S. Granzer, T. Grosvenor, S. Jenness, T. Koratkar, A. Lehner, M. Mottram, C. Naylor, T. Saunders, E. Solomos, N. Steele, I. Tuparev, G. Vestrand, T. White, R. Yost, S. TI A protocol standard for heterogeneous telescope networks SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE instrumentation : miscellaneous; techniques : miscellaneous; methods : observational; telescopes; standards AB The scientific need for a standard protocol permitting the exchange of generic observing services is rapidly escalating as more observatories adopt service observing as a standard operating mode and as more remote or robotic telescopes are brought on-line. To respond to this need, we present the results of the first interoperability workshop for Heterogeneous Telescope Networks (HTN) held in Exeter. We present a draft protocol, designed to be independent of the specific instrumentation and software that controls the remote and/or robotic telescopes, allowing these telescopes to appear to the user with a unified interface despite any underlying architectural differences. (c) 2006 WILEY-VCH Verlag GmbH &Co. KGaA, Weinheim. C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. Teleskoptech Halfmann, D-86356 Neusass Vogelsang, Germany. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Joint Astron Ctr, Hilo, HI 96720 USA. Queens Univ Belfast, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland. Latterfrosken Software Dev Ltd, Walsall WS1 3QA, W Midlands, England. Jackson State Univ, Jackson, MS 39217 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Catonsville, MD 21228 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hellen Naval Acad, Phys Sector, Piraeus 18503, Greece. Natl Astron Ctr, Ainos Mt, Kefallinia Isla, Greece. Tuparev Technol Inc, Sofia 1612, Bulgaria. Los Alamos Natl Lab, Los Alamos, NM 87544 USA. Univ Michigan, Randall Lab, ROTSE, Ann Arbor, MI 48109 USA. RP Allan, A (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM aa@astro.ex.ac.uk RI Naylor, Tim /A-9465-2015; OI Economou, Frossie/0000-0002-8333-7615; Jenness, Tim/0000-0001-5982-167X NR 2 TC 12 Z9 12 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 8 BP 744 EP 750 DI 10.1002/asna.200610625 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600002 ER PT J AU White, RR Allan, A Barthelmy, S Bloom, J Graham, M Hessman, FV Marka, S Rots, A Scholberg, K Seaman, R Stoughton, C Vestrand, WT Williams, R Wozniak, PR AF White, R. R. Allan, A. Barthelmy, S. Bloom, J. Graham, M. Hessman, F. V. Marka, S. Rots, A. Scholberg, K. Seaman, R. Stoughton, C. Vestrand, W. T. Williams, R. Wozniak, P. R. TI Astronomical network event and observation notification SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE instrumentation : miscellaneous; methods : observational; standards; telescopes ID TELESCOPES; SKY AB Networks are becoming a key element in most current and all future, telescope and observatory projects. The ability to easily and efficiently pass observation data, alert data and instrumentation requests between distributed systems could enable science as never before. However, any effective large scale or meta-network of astronomical resources will require a common communication format or development resources will have to be continuously dedicated to creating interpreters. The necessary elements of any astronomy communication can be easily identified, efficiently described and rigidly formatted so that both robotic and human operations can use the same data. In this paper we will explore the current state of notification, what notification requirements are essential to create a successful standard and present a standard now under development by the International Virtual Observatory Alliance (IVOA), called the VOEvent. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Exeter, Exeter, Devon, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. CALTECH, Pasadena, CA 91125 USA. Univ Gottingen, D-3400 Gottingen, Germany. Columbia Univ, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Duke Univ, Durham, NC 27706 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Fermilab Natl Accelerator Lab, Chicago, IL USA. RP White, RR (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM rwhite@lanl.gov RI Barthelmy, Scott/D-2943-2012; OI Rots, Arnold/0000-0003-2377-2356; Wozniak, Przemyslaw/0000-0002-9919-3310 NR 7 TC 8 Z9 8 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 8 BP 775 EP 778 DI 10.1002/asna.200610631 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600008 ER PT J AU Lehner, MJ Alcock, C Axelrod, T Bianco, F Byun, YI Chen, WP Cook, KH Dave, R de Pater, I Giammarco, J King, SK Lee, T Lissauer, J Marshall, SL Mondal, S Nihei, T Rice, J Schwamb, M Wang, A Wang, SY Wen, CY Zhang, ZW AF Lehner, M. J. Alcock, C. Axelrod, T. Bianco, F. Byun, Y. -I. Chen, W. -P. Cook, K. H. Dave, R. de Pater, I. Giammarco, J. King, S. -K. Lee, T. Lissauer, J. Marshall, S. L. Mondal, S. Nihei, T. Rice, J. Schwamb, M. Wang, A. Wang, S. -Y. Wen, C. -Y. Zhang, Z. -W. TI TAOS - The Taiwanese-American Occultation Survey SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE Kuiper Belt; occultations; methods : observational; telescopes ID KUIPER-BELT OBJECTS; BODIES AB The Taiwanese-American Occultation Survey (TAOS) seeks to determine the number and size spectrum for small (similar to 3 km) bodies in the Kuiper Belt. This will be accomplished by searching for the brief occultations of bright stars (R similar to 14) by these objects. We have designed and built a special purpose photometric monitoring system for this purpose. TAOS comprises four 50 cm telescopes, each equipped with a 2048 x 2048 pixel CCD camera, in a compact array located in the central highlands of Taiwan. TAOS will monitor up to 2 000 stars at 5 Hz. The system went into scientific operation in the autumn of 2005. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Yonsei Univ, Dept Astron, Seoul 120749, South Korea. Natl Cent Univ, Inst Astron, Taoyuan 320, Taiwan. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Natl Taiwan Univ, Condensed Matter Sci & Phys Dept, Taipei 106, Taiwan. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. RP Lehner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mlehner@cfa.harvard.edu RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985 NR 7 TC 5 Z9 5 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 8 BP 814 EP 817 DI 10.1002/asna.200610688 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600018 ER PT J AU Tucker, DL Kent, S Richmond, MW Annis, J Smith, JA Allam, SS Rodgers, CT Stute, JL Adelman-McCarthy, JK Brinkmann, J Doi, M Finkbeiner, D Fukugita, M Goldston, J Greenway, B Gunn, JE Hendry, JS Hogg, DW Ichikawa, SI Ivezic, Z Knapp, GR Lampeitl, H Lee, BC Lin, H Mckay, TA Merrelli, A Munn, JA Neilsen, EH Newberg, HJ Richards, GT Schlegel, DJ Stoughton, C Uomoto, A Yanny, B AF Tucker, D. L. Kent, S. Richmond, M. W. Annis, J. Smith, J. A. Allam, S. S. Rodgers, C. T. Stute, J. L. Adelman-McCarthy, J. K. Brinkmann, J. Doi, M. Finkbeiner, D. Fukugita, M. Goldston, J. Greenway, B. Gunn, J. E. Hendry, J. S. Hogg, D. W. Ichikawa, S. -I. Ivezic, Z. Knapp, G. R. Lampeitl, H. Lee, B. C. Lin, H. McKay, T. A. Merrelli, A. Munn, J. A. Neilsen, E. H., Jr. Newberg, H. J. Richards, G. T. Schlegel, D. J. Stoughton, C. Uomoto, A. Yanny, B. TI The Sloan Digital Sky Survey Monitor Telescope Pipeline SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE methods : data analysis; techniques : image processing; techniques : photometric; surveys ID SPECTROSCOPIC TARGET SELECTION; DATA RELEASE; STANDARD STARS; GALAXY SAMPLE; SYSTEM; PHOTOMETRY; SDSS; REPRESENTATIONS; PROGRAM; CATALOG AB The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi-step process which involves data from three different telescopes: the 1.0-m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5-m Photometric Telescope (PT) at the Apache Point Observatory (APO), New Mexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5-m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single-CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0-m and the PT). We also describe transformation equations that convert photometry on the USNO-1.0m u ' g ' r ' i ' z ' system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi-automated PT factory, which runs MTPIPE in the day-to-day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS-related projects, including the Southern u ' g ' r ' i ' z ' Standard Star project, the u ' g ' r ' i ' z ' Open Star Clusters project, and the SDSS extension (SDSS-II). (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37044 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Apache Point Observ, Sunspot, NM 88349 USA. Univ Tokyo, Inst Astron, Sch Sci, Mitaka, Tokyo 1810015, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. NYU, Dept Phys, New York, NY 10003 USA. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15232 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. USN Observ, Flagstaff Stn, Flagstaff, AZ 86002 USA. Rensselaer Polytech Inst, Dept Phys, Troy, NY 12180 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Tucker, DL (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. EM dtucker@fnal.gov RI McKay, Timothy/C-1501-2009; OI McKay, Timothy/0000-0001-9036-6150; Hogg, David/0000-0003-2866-9403; Tucker, Douglas/0000-0001-7211-5729 NR 52 TC 308 Z9 309 U1 1 U2 7 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 9 BP 821 EP 843 DI 10.1002/asna.200610655 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 101ZV UT WOS:000241781300001 ER PT J AU Guainazzi, M Siemiginowska, A Stanghellini, C Grandi, P Piconcelli, E Ugwoke, CA AF Guainazzi, M Siemiginowska, A Stanghellini, C Grandi, P Piconcelli, E Ugwoke, CA TI A hard X-ray view of giga-hertz peaked spectrum radio galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : jets; galaxies : quasars : individual : COINSJ0029+3456, PKS 0500+019, PKS 0941-080, KS2128+048; X-ray : galaxies ID COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; XMM-NEWTON; ASTRONOMICAL DATA; COMPLETE SAMPLE; HOST GALAXIES; QUASARS; GHZ; EMISSION; IDENTIFICATIONS AB We present the first broadband X- ray observations of four Giga- Hertz Peaked Spectrum ( GPS) radio galaxies at redshift less than or similar to 1 performed by Chandra and XMM- Newton. These observations more than double the number of members of this class with measured spectra in hard ( E > 2 keV) X- rays. All sources were detected. Their radio- to- X- ray spectral energy distributions are similar, except for PKS 0941- 080, which is X- ray under- luminous by about two orders of magnitude. The comparison between the full sample of GPS galaxies with measurements in hard X- rays and a control sample of radio galaxies rules out intrinsic X- ray weakness as causing a lower detection rate of GPS sources in X- ray surveys. Four out of seven GPS galaxies exhibit high X- ray column densities, whereas for the remaining three this measurement is hampered by the poor spectral statistics. Bearing in mind the low number statistics in both the GPS and the control sample, the average column density measured in GPS galaxies is larger than in FRI or Broad Line Region FR II radio galaxies, but consistent with that measured in High-Excitation FR II galaxies. This leads to a location the absorbing gas in an obscuring " torus", which prevents us from observing the nuclear region along lines- of- sight perpendicular to the radio axis. This interpretation is supported by the discovery of rapid (timescale similar to 10(3) s) X-ray variability in the GPS galaxy COINSJ0029+ 3456, and by an almost order- of- magnitude difference between the HI column density measured in radio and X- rays in PKS 0500+019. C1 ESA, European Space Astron Ctr, E-28080 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. INAF, Ist Radioastron, I-40129 Bologna, Italy. INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy. RP Guainazzi, M (reprint author), ESA, European Space Astron Ctr, Apartado 50727, E-28080 Madrid, Spain. EM Matteo.Guainazzi@sciops.esa.int OI piconcelli, enrico/0000-0001-9095-2782; Stanghellini, Carlo/0000-0002-6415-854X; Grandi, Paola/0000-0003-1848-6013 NR 79 TC 40 Z9 40 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 JAN PY 2006 VL 446 IS 1 BP 87 EP 96 DI 10.1051/0004-6361:20053374 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001LF UT WOS:000234533900008 ER PT J AU Rodmann, J Henning, T Chandler, CJ Mundy, LG Wilner, DJ AF Rodmann, J Henning, T Chandler, CJ Mundy, LG Wilner, DJ TI Large dust particles in disks around T Tauri stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : pre-main sequence; stars : planetary systems : protoplanetary disks; planetary systems : formation ID YOUNG STELLAR OBJECTS; AURIGA MOLECULAR CLOUD; CIRCUMSTELLAR GAS; IMAGING SURVEY; MASS-LOSS; PROTOPLANETARY DISKS; FORMING REGIONS; SINGLE-STAR; GG TAURI; HL TAURI AB We present 7-mm continuum observations of 14 low-mass pre-main-sequence stars in the Taurus-Auriga star-forming region obtained with the Very Large Array with similar to 1."5 resolution and similar to 0.3 mJy rms sensitivity. For 10 objects, the circumstellar emission has been spatially resolved. The large outer disk radii derived suggest that the emission at this wavelength is mostly optically thin. The millimetre spectral energy distributions are characterised by spectral indices alpha(mm) = 2.3 to 3.2. After accounting for contributions from free-free emission and corrections for optical depth, we determine dust opacity indices beta in the range 0.5 to 1.6, which suggest that millimetre-sized dust aggregates are present in the circumstellar disks. Four of the sources with beta > 1 may be consistent with submicron-sized dust as found in the interstellar medium. Our findings indicate that dust grain growth to millimetre-sized particles is completed within less than 1 Myr for the majority of circumstellar disks. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodmann, J (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM rodmann@mpia.de NR 66 TC 151 Z9 152 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 JAN PY 2006 VL 446 IS 1 BP 211 EP 221 DI 10.1051/0004-6361:20054038 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001LF UT WOS:000234533900017 ER PT J AU Persi, P Tapia, M Smith, HA AF Persi, P Tapia, M Smith, HA TI Mid-infrared images of the massive star forming region W75N SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : formation; infrared : stars; ISM : clouds; ISM : HII regions ID YOUNG STELLAR OBJECTS; SPITZER-SPACE-TELESCOPE; ARRAY CAMERA IRAC; INFRARED OBSERVATIONS; PHOTOMETRY; EMISSION; OUTFLOW; COLORS; CLOUD; DUST AB An infrared study that includes ground-based mid-infrared images between 8.7 and 18.7 mu m and IRAC images at 3.6, 4.5, 5.8 and 8.0 mu m of the W75 N massive star forming region is presented. The 12.5 mu m image shows the presence of four mid-infrared sources in the region W75 N( B), three of which have bright near-infrared counterparts, IRS 1, IRS 2 and IRS 3, all with significant excess emission at lambda > 2.0 mu m. IRS 2 has a steep energy distribution and the computed infrared luminosity is consistent with the presence of a young B3 star. The observed IRAC colors of IRS 3 indicate that this source is a Class II intermediate mass young star, consistent with its infrared energy distribution and luminosity. The fourth, newly discovered, mid-infrared source appears coincident with the ultracompact HII region VLA 3, and is located within the millimeter core MM 1. We derived a luminosity of similar to 750 L-circle dot and a visual extinction A(V) similar or equal to 90 for this source. From the IRAC images, we detected 75 sources in an area of 120" x 120" centered in W75 N. At least 25 of these sources are associated with the molecular cloud and form a young stellar cluster as shown in the IRAC two-color and the H - K-s versus K-s - [3.6] diagrams. C1 Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22830, Baja California, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ist Astrofis Spaziale & Fis Cosm, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM persi@rm.iasf.cnr.it OI Tapia, Mauricio/0000-0002-0506-9854 NR 26 TC 14 Z9 14 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2006 VL 445 IS 3 BP 971 EP 978 DI 10.1051/0004-6361:20053251 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999QH UT WOS:000234404500024 ER PT J AU Greene, JE Ho, LC Ulvestad, JS AF Greene, JE Ho, LC Ulvestad, JS TI The radio quiescence of active galaxies with high accretion rates SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : jets; galaxies : nuclei; galaxies : Seyfert; galaxies : structure; radio continuum : galaxies ID NARROW-LINE SEYFERT-1; BLACK-HOLE MASS; BRIGHT QUASAR SURVEY; DIGITAL SKY SURVEY; X-RAY BINARIES; GALACTIC NUCLEI; ENERGY-DISTRIBUTIONS; DOMINATED ACCRETION; PHYSICAL DRIVERS; EDDINGTON RATIO AB We present 6 cm Very Large Array observations of the Greene & Ho sample of 19 low-mass active galaxies with high accretion rates. This is one of the only studies of a uniform sample of narrow-line Seyfert 1 ( NLS1) galaxies with such high sensitivity and resolution. Although we detect only one source, the entire sample is very radio quiet down to strong limits. GH10 was found to have a radio power of 8.5 x 10(21) W Hz(-1) and a ratio R equivalent to f(6 cm)/f(4400) ((A) over circle) of 2.8. The 3 sigma upper limits for the remaining nondetections correspond to radio powers from 3 x 10(20) to 8 x 10(21) W Hz(-1) and 0.47 < R < 9.9. Stacking all nondetections yields an even stronger upper limit of R <= 0.27. An assessment of existing observations in the literature confirms our finding that NLS1s are consistently radio-quiet, with a radio-loud fraction of 0% - 6%, which is significantly lower than the 10% - 20% observed in the general quasar population. By analogy with stellar mass black holes, we argue that AGNs undergo a state transition at L-bol/L-Edd approximate to 0.01. Below this value a radiatively inefficient accretion flow effectively drives an outflow, which disappears when the flow turns into an optically thick, geometrically thin disk, or a radiation pressure - dominated slim disk at still higher L-bol/L-Edd. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Greene, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Ulvestad, James/0000-0002-9362-7237 NR 98 TC 59 Z9 59 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 JAN 1 PY 2006 VL 636 IS 1 BP 56 EP 62 DI 10.1086/497905 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800006 ER PT J AU Madejski, G Done, C Zycki, PT Greenhill, L AF Madejski, G Done, C Zycki, PT Greenhill, L TI X-Ray emission from megamaser galaxy IC 2560 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (IC 2560); masers; X rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; WATER MASER EMISSION; K-ALPHA LINE; ACCRETION DISK; CIRCINUS GALAXY; H2O MEGAMASERS; BLACK-HOLE; XMM-NEWTON; IRON AB An observation of the H2O megamaser galaxy IC 2560 with the Chandra X-Ray Observatory reveals a complex spectrum composed of soft X-ray emission due to multitemperature thermal plasma and a hard continuum with strong emission lines. The continuum is most likely a Compton reflection ( reprocessing) of primary emission that is completely absorbed at least up to 7 keV. The lines can be identified with fluorescence from Si, S, and Fe in the lowest ionization stages. The equivalent widths of the Si and S lines are broadly compatible with those anticipated for reprocessing by optically thick cold plasma of solar abundances, while the large equivalent width of the Fe line requires some overabundance of iron. A contribution to the line from a transmitted component cannot be ruled out, but the limits on the strength of the Compton shoulder make it less likely. From the bolometric luminosity of the nuclear region, we infer that the source radiates at 1% - 10% of its Eddington luminosity for an adopted central mass of 3 x 10(6) M-circle dot. The overall spectrum is consistent with the hypotheses that the central engines powering the detected megamasers in accretion disks are obscured from direct view by the associated accretion disk material itself and that there is a correlation between the occurrence of megamaser emission and Compton-thick absorption columns. For the 11 known galaxies with both column density measurements and maser emission believed to arise from accretion disks, eight AGNs are Compton thick. C1 Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. Univ Durham, Dept Phys, Durham, England. Nicolaus Copernicus Astron Ctr, Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Madejski, G (reprint author), Stanford Linear Accelerator Ctr, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. EM madejski@stanford.edu RI done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 NR 57 TC 19 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 JAN 1 PY 2006 VL 636 IS 1 BP 75 EP 82 DI 10.1086/497894 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800008 ER PT J AU Baldi, A Raymond, JC Fabbiano, G Zezas, A Rots, AH Schweizer, F King, AR Ponman, TJ AF Baldi, A Raymond, JC Fabbiano, G Zezas, A Rots, AH Schweizer, F King, AR Ponman, TJ TI Chemical enrichment of the complex hot ISM of the antennae galaxies. II. Physical properties of the hot gas and supernova feedback SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038/4039); galaxies : interactions; galaxies : peculiar; X-rays : galaxies; X-rays : ISM ID X-RAY-EMISSION; YOUNG STAR-CLUSTERS; INTRACLUSTER MEDIUM ENRICHMENT; HUBBLE-SPACE-TELESCOPE; ON STARBURST GALAXIES; INTERSTELLAR-MEDIUM; CHANDRA OBSERVATIONS; INTERGALACTIC MEDIUM; GALACTIC WINDS; NGC 4038/4039 AB We investigate the physical properties of the interstellar medium ( ISM) in the merging pair of galaxies known as the Antennae ( NGC 4038/ 4039), using the deep co-added similar to 411 ks Chandra ACIS-S data set. The method of analysis and some of the main results from the spectral analysis, such as metal abundances and their variations from similar to 0.2 to similar to 20 - 30 times solar, are described in Paper I ( Baldi et al.). In the present paper we investigate in detail the physics of the hot emitting gas, deriving measures for the hot gas mass ( similar to 10(7) M-circle dot), cooling times ( 10(7) - 10(8) yr), and pressure ( 3.5 x 10(-11) -2.8 x 10(-10) dyne cm(-2)). In at least one of the two nuclei ( NGC 4038), the hot gas pressure is significantly higher than the CO pressure, implying that shock waves may be driven into the CO clouds. Comparison of the metal abundances with the average stellar yields predicted by theoretical models of SN explosions points to SNe of Type II as the main contributors of metals to the hot ISM. There is no evidence of any correlation between radio-optical star formation indicators and the measured metal abundances. Although due to uncertainties in the average gas density we cannot exclude that mixing may have played an important role, the short time required to produce the observed metal masses ( less than or similar to 2 Myr) suggests that the correlations are unlikely to have been destroyed by efficient mixing. More likely, a significant fraction of Type II SN ejecta may be in a cool phase, in grains, or escaping in hot winds. In each case, any such fraction of the ejecta would remain undetectable with soft X-ray observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie, Pasadena, CA 91101 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abaldi@cfa.harvard.edu; jraymond@cfa.harvard.edu; pepi@cfa.harvard.edu; azezas@cfa.harvard.edu; arots@cfa.harvard.edu; schweizer@ociw.edu; ark@astro.le.ac.uk; tjp@star.sr.bham.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 61 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 158 EP 171 DI 10.1086/497880 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800015 ER PT J AU Magnani, L Zelenik, S Dame, TM Engebreth, B AF Magnani, L Zelenik, S Dame, TM Engebreth, B TI CH 3 GHz observations of the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; ISM : molecules; radio lines : ISM ID DENSE INTERSTELLAR CLOUDS; GROUND-STATE TRANSITIONS; H-2 CONVERSION FACTOR; CENTER REGION; MOLECULAR CLOUDS; MILKY-WAY; CO SURVEY; TRANSLUCENT CLOUDS; RADIO OBSERVATIONS; DIFFUSE AB A 3; 3 map of the Galactic center was made at 90 resolution and 100 spacing in the CH (II1/2)-I-2, J = (1/2), F = 1-1 transition at 3335 MHz. The CH emission shows a velocity extent that is close to that of the CO( 1-0) line, but the CH line profiles differ markedly from the CO. The 3335 MHz CH transition primarily traces low-density molecular gas in the high-density, high-pressure environment of the Galactic center interstellar medium. If the empirical N( CH)-N( H-2) relation derived for molecular clouds in the disk is valid at the Galactic center, then our observations indicate that the mass of the low-density component within similar to 30 pc of the Galactic center is similar to 9 x 10(6) M-circle dot. The CO-H-2 conversion factor obtained for the low-density gas in the mapped region is greater than that thought to apply to the dense molecular gas at the Galactic center. The CH spectra show evidence of emission from molecular clouds along the line of sight in both the foreground and the background. The scale height of these clouds ranges from 27 to 109 pc, consistent with previous work based on observations of molecular clouds in the inner Galaxy. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. RP Magnani, L (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. NR 54 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 267 EP 274 DI 10.1086/497949 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800022 ER PT J AU Beuther, H Zhang, Q Reid, MJ Hunter, TR Gurwell, M Wilner, D Zhao, JH Shinnaga, H Keto, E Ho, PTP Moran, JM Liu, SY AF Beuther, H Zhang, Q Reid, MJ Hunter, TR Gurwell, M Wilner, D Zhao, JH Shinnaga, H Keto, E Ho, PTP Moran, JM Liu, SY TI Submillimeter array 440 mu m/690 GHz line and continuum observations of Orion KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual ( Orion KL); ISM : lines and bands; ISM : molecules; stars : formation; submillimeter; techniques : interferometric ID MARYLAND-ASSOCIATION ARRAY; MIXED VERTICAL PROFILE; STAR-FORMING REGION; HOT CORE; APERTURE SYNTHESIS; MOLECULAR CLOUD; METHYL CYANIDE; MILLIMETER; RESOLUTION; TITAN AB Submillimeter Array observations of Orion KL at similar to 1 '' resolution in the 440 mu m/690 GHz band reveal new insights about the continuum and line emission of the region. The 440 mu m continuum flux density measurement from source I allows us to differentiate among the various proposed physical models. Source I can be well modeled by a '' normal '' protostellar spectral energy distribution (SED) consisting of a proton-electron free-free emission component at low frequencies and a strong dust component in the submillimeter bands. Furthermore, we find that the protostellar object SMA1 is clearly distinct from the hot core. The nondetection of SMA1 at centimeter and infrared wavelengths suggests that it may be one of the youngest sources in the entire Orion KL region. The molecular line maps show emission mainly from source I, SMA1, and the hot core peak position. An analysis of the CH(3)CN(37(K)-36(K)) K-ladder (K = 0,...,3) indicates a warm gas component of the order of 600 +/- 200 K. In addition, we detect a large fraction (similar to 58%) of unidentified lines and discuss the difficulties of line identification at these frequencies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu NR 37 TC 39 Z9 39 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 323 EP 331 DI 10.1086/498015 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800027 ER PT J AU Pease, DO Drake, JJ Kashyap, VL AF Pease, DO Drake, JJ Kashyap, VL TI The darkest bright star: Chandra X-ray observations of Vega SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : activity; stars : coronae; stars : early-type; stars : individual (Vega, alpha Lyrae); X-rays : stars ID HERBIG AE/BE STARS; CHEMICALLY PECULIAR STARS; EMISSION; CALIBRATION; COMPANIONS; TELESCOPE; PLEIADES; CORONAE; COUNTS; ROSAT AB We present X-ray observations of Vega obtained with the Chandra High Resolution Camera and Advanced CCD Imaging Spectrometer. After a total of 29 ks of observation with Chandra, X-rays from Vega remain undetected. We derive upper limits to the X-ray luminosity of Vega as a function of temperature over the range of 10(5) - 10(7) K and find a 99.7% upper limit as low as similar to 2 x 10(25) ergs s(-1) at T = 10(6.2) K. We also compare these new deeper observations with the limit derived from a reanalysis of ROSAT PSPC data. Our X-ray luminosity limit for Vega is still greater than predictions of post-Herbig Ae phase X-rays from the shear dynamo model proposed by Tout & Pringle for a Vega age of 350 Myr. If the age of Vega is closer to 100 Myr, as suggested by some indicators, our X-ray limit is then similar to Tout-Pringle model predictions. Current X-ray observations of Vega are therefore unable to discriminate between different scenarios explaining the X-ray activity of the convectively stable Herbig Ae/Be stars. Further progress is more likely to be achieved through X-ray observations of younger main-sequence early-type A stars, whose conjectured residual post-Herbig Ae phase X-ray activity would be significantly higher. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Pease, DO (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-83, Cambridge, MA 02138 USA. EM dpease@cfa.harvard.edu; jdrake@cfa.harvard.edu; vkashyap@cfa.harvard.edu NR 44 TC 13 Z9 13 U1 0 U2 0 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 JAN 1 PY 2006 VL 636 IS 1 BP 426 EP 431 DI 10.1086/497888 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800036 ER PT J AU Charbonneau, D Winn, JN Latham, DW Bakos, G Falco, EE Holman, MJ Noyes, RW Csak, B Esquerdo, GA Everett, ME O'Donovan, FT AF Charbonneau, D Winn, JN Latham, DW Bakos, G Falco, EE Holman, MJ Noyes, RW Csak, B Esquerdo, GA Everett, ME O'Donovan, FT TI Transit photometry of the core-dominated planet HD 149026b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (HD 149026); techniques : photometric ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; INFRARED OBSERVATIONS; SECONDARY ECLIPSE; GALACTIC DISK; GIANT PLANET; PARENT STAR; 209458B AB We report g, V, and r photometric time series of HD 149026 spanning predicted times of transit of the Saturn-mass planetary companion, which was recently discovered by Sato and collaborators. We present a joint analysis of our observations and the previously reported photometry and radial velocities of the central star. We refine the estimate of the transit ephemeris to T-c = (2, 453, 527.87455(-0.00091)(+0.00085)) + (2.87598(-0.00017)(+0.00012))N (HJD). Assuming that the star has a radius of 1: 45 +/- 0.10 R-circle dot and a mass of 1.30 +/- 0.10 M-circle dot, we estimate the planet radius to be (0.726 +/- 0.064)R-Jup, which implies a mean density of 1.07(-0.30)(+0.42) g cm(-3). This density is significantly greater than predicted for models that include the effects of stellar insolation and in which the planet has only a small core of solid material. Thus, we confirm that this planet likely contains a large core and that the ratio of core mass to total planet mass is more akin to that of Uranus and Neptune than to either Jupiter or Saturn. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Planetary Sci Inst, Tucson, AZ 85719 USA. CALTECH, Pasadena, CA 91125 USA. RP Charbonneau, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dcharbonneau@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X NR 50 TC 56 Z9 56 U1 0 U2 0 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 JAN 1 PY 2006 VL 636 IS 1 BP 445 EP 452 DI 10.1086/497959 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800038 ER PT J AU Goodman, J Narayan, R AF Goodman, J Narayan, R TI Fitting formula for flux scintillation of compact radio sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; radio continuum : general; scattering ID GAMMA-RAY-BURST; SCATTER-BROADENED IMAGE; INTERSTELLAR SCINTILLATION; ANNUAL MODULATION; SPECTRUM; VARIABILITY; PLASMA; SIZE; PROPAGATION; AFTERGLOW AB We present a fitting function to describe the statistics of flux modulations caused by interstellar scintillation. The function models a very general quantity: the cross-correlation of the flux observed from a compact radio source of finite angular size observed at two frequencies and at two positions or times. The formula will be useful for fitting data from sources such as intraday variables and gamma-ray burst afterglows. These sources are often observed at relatively high frequencies (several gigahertz), where interstellar scattering is neither very strong nor very weak, so that asymptotic formulae are inapplicable. C1 Princeton Univ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Goodman, J (reprint author), Princeton Univ, Princeton, NJ 08544 USA. EM jeremy@astro.princeton.edu; narayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 31 TC 12 Z9 12 U1 0 U2 0 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 JAN 1 PY 2006 VL 636 IS 1 BP 510 EP 527 DI 10.1086/497903 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800043 ER PT J AU Brickhouse, NS Schmelz, JT AF Brickhouse, NS Schmelz, JT TI The transparency of solar coronal active regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; scattering; stars : coronae; Sun : corona; Sun : UV radiation; Sun : X-rays, gamma rays ID SPECTRAL-LINE INTENSITIES; X-RAY OBSERVATIONS; FE-XVII; RELATIVE INTENSITY; STELLAR CORONAE; MAXIMUM-MISSION; OPTICALLY THIN; ATOMIC DATA; EMISSION; RATIOS AB Resonance scattering has often been invoked to explain the disagreement between the observed and predicted line ratios of Fe XVII lambda 15.01 to Fe XVII lambda 15.26 ( the "3C/3D" ratio). In this process photons of lambda 15.01, with its much higher oscillator strength, are preferentially scattered out of the line of sight, thus reducing the observed line ratio. Recent laboratory measurements, however, have found significant inner-shell Fe XVI lines at 15.21 and 15.26, suggesting that the observed 3C/3D ratio results from blending. Given our new understanding of the fundamental spectroscopy, we have reexamined the original solar spectra, identifying the Fe XVI lambda 15.21 line and measuring its flux to account for the contribution of Fe XVI to the lambda 15.26 flux. Deblending brings the 3C/3D ratio into good agreement with the experimental ratio; hence, we find no need to invoke resonance scattering. Low opacity in Fe XVII lambda 15.01 also implies low opacity for Fe XV lambda 284.2, ruling out resonance scattering as the cause of the fuzziness of TRACE and SOHO-EIT 284 images. The images must, instead, be unresolved due to the large number of structures at this temperature. Insignificant resonance scattering implies that future instruments with higher spatial resolution could resolve the active region plasma into its component loop structures. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbrickhouse@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 NR 37 TC 27 Z9 28 U1 0 U2 1 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 JAN 1 PY 2006 VL 636 IS 1 BP L53 EP L56 DI 10.1086/500045 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100014 ER PT J AU Fuentes, CI Stanek, KZ Gaudi, BS McLeod, BA Bogdanov, S Hartman, JD Hickox, RC Holman, MJ AF Fuentes, CI Stanek, KZ Gaudi, BS McLeod, BA Bogdanov, S Hartman, JD Hickox, RC Holman, MJ TI The hypervelocity star SDSS J090745.0+024507 is variable SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; stellar dynamics ID PULSATING B-STARS; GALACTIC-CENTER; BLACK-HOLE; SPACED DATA; DISCOVERY; VELOCITY; GALAXY; HALO AB We present high-precision photometry of the hypervelocity star SDSS J090745.0 +/- 024507 (hereafter HVS), which has a Galactic rest-frame radial velocity of v = 709 km s(-1), and thus has likely been ejected from the supermassive black hole in the Galactic center. Our data were obtained on two nights using the MMT 6.5 m telescope and is supplemented by lower precision photometry obtained on four nights using the FLWO 1.2 m telescope. The high-precision photometry indicates that the HVS is a low-amplitude variable. Assuming a periodic, sinusoidal model for this variation, we obtain period P = 0.2-2 days and amplitude A = 2%-10%. Together with the known effective temperature of T(eff) similar or equal to 10,500 K (spectral type B9), this variability implies that the HVS is probably a MS star, since BHB stars do not appear to be variable. Thus, we resolve the previously reported twofold degeneracy in the luminosity and distance of the star. The variability, effective temperature, and possible periodicity of the HVS indicate that it likely belongs to the class of slowly pulsating B-type main-sequence stars. The HVS has a heliocentric distance of 71 kpc and an age of <= 0.35 Gyr. The time of ejection from the center of the Galaxy is <= 100 Myr, and thus the existence of the HVS constitutes observational evidence of a population of young stars in the proximity of the central supermassive black hole similar to 0.1 Gyr ago. It is possible that the HVS was a member of a binary that was tidally disrupted by the central black hole; we discuss constraints on the properties of the companion's orbit. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fuentes, CI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cfuentes@cfa.harvard.edu; kstanek@cfa.harvard.edu; sgaudi@cfa.harvard.edu; bmcleod@cfa.harvard.edu; sbogdano@cfa.harvard.edu; jhartman@cfa.harvard.edu; rhickox@cfa.harvard.edu; mholman@cfa.harvard.edu RI Gaudi, Bernard/I-7732-2012; Fuentes, Cesar /G-7506-2016; OI Bogdanov, Slavko/0000-0002-9870-2742; Hartman, Joel/0000-0001-8732-6166 NR 27 TC 28 Z9 28 U1 0 U2 1 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 JAN 1 PY 2006 VL 636 IS 1 BP L37 EP L40 DI 10.1086/499233 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100010 ER PT J AU Teixeira, PS Lada, CJ Young, ET Marengo, M Muench, A Muzerolle, J Siegler, N Rieke, G Hartmann, L Megeath, ST Fazio, G AF Teixeira, PS Lada, CJ Young, ET Marengo, M Muench, A Muzerolle, J Siegler, N Rieke, G Hartmann, L Megeath, ST Fazio, G TI Identifying primordial substructure in NGC 2264 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; open clusters and associations : individual (NGC 2264); stars : formation; stars : pre-main-sequence ID MULTIBAND IMAGING PHOTOMETER; OB1 MOLECULAR CLOUD; STAR-FORMATION; CLUSTER; SPITZER; FLOWS; EMISSION AB We present new Spitzer Space Telescope observations of the young cluster NGC 2264. Observations at 24 mm with the Multiband Imaging Photometer have enabled us to identify the most highly embedded and youngest objects in NGC 2264. This Letter reports on one particular region of NGC 2264 where bright 24 mm sources are spatially configured in curious linear structures with quasi-uniform separations. The majority of these sources (similar to 60%) are found to be protostellar in nature, with Class I spectral energy distributions. Comparison of their spatial distribution with submillimeter data from Wolf-Chase et al. and millimeter data from Peretto et al. shows a close correlation between the dust filaments and the linear spatial configurations of the protostars, indicating that star formation is occurring primarily within dense, dusty filaments. Finally, the quasi-uniform separations of the protostars are found to be comparable in magnitude to the expected Jeans length, suggesting thermal fragmentation of the dense filamentary material. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Lisbon, Fac Ciencias, Dept Fis, P-1749016 Lisbon, Portugal. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Teixeira, PS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pteixeira@cfa.harvard.edu RI Teixeira, Paula Stella/O-2289-2013; OI Teixeira, Paula Stella/0000-0002-3665-5784; Muench, August/0000-0003-0666-6367 NR 23 TC 72 Z9 72 U1 0 U2 1 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 JAN 1 PY 2006 VL 636 IS 1 BP L45 EP L48 DI 10.1086/500009 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100012 ER PT J AU van der Wel, A Franx, M van Dokkum, PG Huang, J Rix, HW Illingworth, GD AF van der Wel, A Franx, M van Dokkum, PG Huang, J Rix, HW Illingworth, GD TI The evolution of rest-frame K-band properties of early-type galaxies from z=1 to the present SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : formation ID FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; POPULATION SYNTHESIS; LUMINOSITY EVOLUTION; STELLAR POPULATIONS; FIELD GALAXIES; SPECTROSCOPY; PHOTOMETRY; COMBO-17; REDSHIFT AB We measure the evolution of the rest-frame K-band fundamental plane from z = 1 to the present by using IRAC imaging of a sample of early-type galaxies in the Chandra Deep Field-South at z similar to 1 with accurately measured dynamical masses. We find that M/L-K evolves as Delta 1n (M/L-K) = (-1.18 +/- 0.10)z, which is slower than in the B band [Delta 1n (M/L-B) = (-1.46 +/- 0.09)z]. In the B band, the evolution has been demonstrated to be strongly mass-dependent. In the K band, we find a weaker trend: galaxies more massive than M = 2 x 10(11) M-circle dot evolve as Delta 1n (M/L-K) = (-1.01 +/- 0.16)z; less massive galaxies evolve as Delta 1n (M/L-K) = (-1.27 +/- 0.11)z. As expected from stellar population models, the evolution in M/L-K is slower than the evolution in M/L-B. However, when we make a quantitative comparison, we find that the single-burst Bruzual-Charlot models do not fit the results well, unless large dust opacities are allowed at z = 1. Models with a flat IMF fit better; Maraston models with a different treatment of AGB stars fit best. These results show that the interpretation of rest-frame near-IR photometry is severely hampered by model uncertainties and therefore that the determination of galaxy masses from rest-frame near-IR photometry may be harder than was thought before. C1 Leiden Observ, NL-2300 AA Leiden, Netherlands. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. RP van der Wel, A (reprint author), Leiden Observ, POB 9513, NL-2300 AA Leiden, Netherlands. RI van der Wel, Arjen/G-8365-2011 NR 32 TC 29 Z9 29 U1 0 U2 1 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 JAN 1 PY 2006 VL 636 IS 1 BP L21 EP L24 DI 10.1086/499919 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100006 ER PT J AU Webb, TMA van Dokkum, P Egami, E Fazio, G Franx, M Gawiser, E Herrera, D Huang, JS Labbe, I Lira, P Marchesini, D Maza, J Quadri, R Rudnick, G van der Werf, P AF Webb, TMA van Dokkum, P Egami, E Fazio, G Franx, M Gawiser, E Herrera, D Huang, JS Labbe, I Lira, P Marchesini, D Maza, J Quadri, R Rudnick, G van der Werf, P TI Star formation in distant red galaxies: Spitzer observations in the Hubble Deep Field-South SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : evolution; galaxies : high-redshift; galaxies : starburst; infrared : galaxies ID HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; SUBSTANTIAL POPULATION; LUMINOSITY DENSITY; RADIO-EMISSION; SOURCE COUNTS; LOCKMAN HOLE; Z-GREATER-THAN-OR-SIMILAR-TO-2; Z-GREATER-THAN-2; PHOTOMETRY AB We present Spitzer 24 mu m imaging of 1.5 < z < 2.5 distant red galaxies (DRGs) in the 10' x 10' extended Hubble Deep Field-South of the Multiwavelength Survey by Yale-Chile. We detect 65% of the DRGs with K-AB < 23.2 mag at S-24 mu m >= 40 mu Jy and conclude that the bulk of the DRG population is dusty active galaxies. A mid-infrared (MIR) color analysis with IRAC data suggests that the MIR fluxes are not dominated by buried AGNs, and we interpret the high detection rate as evidence for a high average star formation rate of < SFR > = 130 +/- 30 M-circle dot yr(-1). From this, we infer that DRGs are important contributors to the cosmic star formation rate density at z similar to 2, at a level of similar to 0.02 M-circle dot yr(-1) Mpc(-3) to our completeness limit of K-AB = 22.9 mag. C1 Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Chile, Dept Astron, Santiago, Chile. Carnegie Inst Washington, Pasadena, CA 91101 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Webb, TMA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Lira, Paulina/G-8536-2016; Maza, Jose/I-5722-2016 OI Maza, Jose/0000-0003-2068-1328 NR 33 TC 41 Z9 41 U1 0 U2 1 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 JAN 1 PY 2006 VL 636 IS 1 BP L17 EP L20 DI 10.1086/499805 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100005 ER PT J AU Baldi, A Raymond, JC Fabbiano, G Zezas, A Rots, AH Schweizer, F King, AR Ponman, TJ AF Baldi, A Raymond, JC Fabbiano, G Zezas, A Rots, AH Schweizer, F King, AR Ponman, TJ TI Chemical enrichment of the complex hot ISM of the Antennae galaxies. I. Spatial and spectral analysis of the diffuse X-ray emission SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : individual (NGC 4038/39); galaxies : interactions; galaxies : peculiar; X-rays : galaxies; X-rays : ISM ID YOUNG STAR-CLUSTERS; CHANDRA OBSERVATIONS; INTERSTELLAR-MEDIUM; NGC 4038/39; MOLECULAR-COMPLEXES; SHOCK-WAVES; NGC-4038/4039; GAS; EVOLUTION; ABUNDANCE AB We present an analysis of the properties of the hot interstellar medium (ISM) in the merging pair of galaxies known as the Antennae (NGC 4038/4039), performed using the deep, co-added similar to 411 ks Chandra ACIS-S data set. These deep X-ray observations and Chandra's high angular resolution allow us to investigate the properties of the hot ISM with unprecedented spatial and spectral resolution. Through a spatially resolved spectral analysis, we find a variety of temperatures (from 0.2 to 0.7 keV) and NH (from Galactic to 2x10(21) cm(-2)). Metal abundances for Ne, Mg, Si, and Fe vary dramatically throughout the ISM from subsolar values (similar to 0.2) up to several times solar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Observ, Pasadena, CA 91101 USA. Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Baldi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abaldi@cfa.harvard.edu; jraymond@cfa.harvard.edu; pepi@cfa.harvard.edu; azezas@cfa.harvard.edu; arots@cfa.harvard.edu; schweizer@ociw.edu; ark@astro.le.ac.uk; tjp@star.sr.bham.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356 NR 43 TC 16 Z9 16 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 JAN PY 2006 VL 162 IS 1 BP 113 EP 133 DI 10.1086/497914 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RS UT WOS:000235130700007 ER PT J AU Viti, S Hartquist, TW Myers, PC AF Viti, Serena Hartquist, Thomas W. Myers, Philip C. TI Chemical telemetry of OH observed to measure interstellar magnetic fields SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE ISM : HII regions; magnetic fields; molecules-masers-stars : formation ID H-II REGIONS; MOLECULAR CLOUDS; METHANOL MASERS; UMIST DATABASE; EVOLUTION; HYDROXYL; MODEL AB We present models for the chemistry in gas moving towards the ionization front of an HII region. When it is far from the ionization front, the gas is highly depleted of elements more massive than helium. However, as it approaches the ionization front, ices are destroyed and species formed on the grain surfaces are injected into the gas phase. Photodissociation removes gas phase molecular species as the gas flows towards the ionization front. We identify models for which the OH column densities are comparable to those measured in observations undertaken to study the magnetic fields in star forming regions and give results for the column densities of other species that should be abundant if the observed OH arises through a combination of the liberation of H2O from surfaces and photodissociation. They include CH3OH, H2CO, and H2S. Observations of these other species may help establish the nature of the OH spatial distribution in the clouds, which is important for the interpretation of the magnetic field results. C1 UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Viti, S (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM sv@star.ucl.ac.uk NR 24 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X EI 1572-946X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2006 VL 302 IS 1-4 BP 109 EP 115 DI 10.1007/s10509-005-9011-x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074VP UT WOS:000239840200013 ER PT J AU Lorenzini, E Bombardelli, C Cosmo, M Harwit, M Leisawitz, D Farley, R Rinehart, S Quinn, D Miller, D AF Lorenzini, Enrico Bombardelli, Claudio Cosmo, Mario Harwit, Martin Leisawitz, David Farley, Rodger Rinehart, Stephen Quinn, David Miller, David TI Far-infrared/submillimeter astronomical interferometry with spaceborne tether formations SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE instrumentation : miscellaneous; space vehicles : miscellaneous; techniques : miscellaneous; astronomical data bases : miscellaneous ID PROBE WMAP OBSERVATIONS; 1ST STARS; SYSTEM; EMISSION; DYNAMICS AB Through the continuing development of improved detectors and detector arrays, far-infrared/submillimeter astronomical space missions have had enormous successes in recent years. Despite these advances, the diffraction-limited angular resolving power has remained virtually constant. The advent of telescopes with apertures of several meters will improve this capability, but will still leave image resolution many orders of magnitude poorer than in most other spectral ranges. Here we point out that the only foreseeable way to improve image quality to rival that of modem optical telescopes will be with interferometers whose light collectors are connected by tethers. After making the scientific case for high spatial resolution far-infrared/submillimeter imaging and the use of interferometry as the most immediate way of producing results, we discuss recent advances in dynamic analysis and control of tethered formations, and argue that the further development and testing of tethers in space is a first step toward providing improved far-infrared/submillimeter angular resolution and astronomical image quality. C1 Cornell Univ, Ithaca, NY USA. Univ Padua, Dept Engn Mech, Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. MIT, Cambridge, MA 02139 USA. RP Harwit, M (reprint author), 511 H St SW, Washington, DC 20024 USA. EM harwit@verizon.net NR 28 TC 10 Z9 10 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2006 VL 302 IS 1-4 BP 225 EP 239 DI 10.1007/s10509-006-9038-7 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074VP UT WOS:000239840200027 ER PT B AU Dupree, AK Ake, TB Brickhouse, NS Hussain, GAJ Jardine, M AF Dupree, A. K. Ake, T. B. Brickhouse, N. S. Hussain, G. A. J. Jardine, M. BE Sonneborn, G Moos, HW Andersson, BG TI AB Dor: Beyond the photosphere SO Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID DORADUS; TOPOLOGY AB FUSE spectra of the strong O VI 1032 angstrom emission in the active dwarf star AB Dor show modulation in both flux and profile with rotational phase that corresponds to regions of open and closed magnetic field in the star's corona. In Dec. 2003, activity appears at mid-latitudes and is confined to similar to 1.3-1.4R(star). These observations provide the first spectroscopic confirmation of the large scale magnetic structures and their dynamics in a stellar corona. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 168 EP 170 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300032 ER PT B AU Lobel, A Avrett, EH Aufdenberg, JP AF Lobel, A. Avrett, E. H. Aufdenberg, J. P. BE Sonneborn, G Moos, HW Andersson, BG TI Semi-empiric radiative transfer modeling of FUSE stellar spectra SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID ALPHA-ORIONIS AB We present an overview of radiative transfer modeling efforts to interpret spectra of a variety of stellar objects observed with FUSE. Detailed radiative transfer modeling of high ion emission line profiles of CIII and OVI observed in the far-UV spectrum, provides a powerful means to probe the thermal and dynamic properties of high-temperature plasmas in the atmospheres of stars. We model asymmetric emission lines of CIII lambda 977 (and MgII h & k) observed in spectra of luminous cool stars such as alpha Aqr, to infertile wind- and microturbulence velocity structures of the upper chromosphere. Semi-empiric radiative transfer models that include transition region temperature conditions, are further developed based on detailed fits to O VI resonance emission lines in the supergiant alpha Aqr, the classical Cepheid variable beta Dor, and to self-absorbed O VI emission lines in the cataclysmic variable SW UMa. We observe that the C in resonance line profile of alpha Aqr assumes a remarkable asymmetric shape, reminiscent of P Cygni type profiles observed in hot luminous supergiants. The model calculations indicate outflow velocities above similar to 140 km s(-1) at kinetic temperatures of 65 kK and higher. Based on detailed model fits to the narrow red-shifted and self-absorbed O VI emission lines of SW UMa we compute that the gas- and electron density exceed the density conditions of the upper solar transition region by about three orders of magnitude. We propose that the large gas density of rho similar or equal to 1.4 10(-11) g cm(-3) favors a region of warm dense plasma of 100 kK <= T-gas <= 300 kK that collapses onto the white dwarf with a mass accretion rate of 1-2 10(15) g s(-1) above or between the accretion disk. We discuss how detailed semi-empiric fits to emission lines observed with the high spectral resolution of FUSE can provide reliable constraints on the mass loss or mass accretion rates in these objects. C1 [Lobel, A.; Avrett, E. H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Aufdenberg, J. P.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Lobel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alobel@cfa.harvard.edu; jasona@noao.edu FU NASA [GI-D107, GI-E068] FX Financial support for this research has been provided by NASA FUSE grants GI-D107 and GI-E068. NR 5 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 171 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300033 ER PT B AU Mathur, S Nicastro, F Williams, R AF Mathur, Smita Nicastro, Fabrizio Williams, Rik BE Sonneborn, G Moos, HW Andersson, BG TI UV and X-ray observations of warm-hot intergalactic medium SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID LOW-REDSHIFT; FOREST AB We present Chandra and FUSE spectra of the line of sight towards Mrk 421. In the Chandra spectrum we detect two intervening systems through absorption lines of highly ionized metals such as O VII. Through detailed modeling, we derive physical conditions in the absorption systems, which are found to be similar to those expected from filaments of warm-hot intergalactic medium. We find that most of the missing baryons at low redshift indeed reside in the warm-hot intergalctic medium. C1 [Mathur, Smita; Williams, Rik] Ohio State Univ, 140 W 18th Ave, Columbus, OH 43210 USA. [Nicastro, Fabrizio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mathur, S (reprint author), Ohio State Univ, 140 W 18th Ave, Columbus, OH 43210 USA. EM smita@astronomy.ohio-state.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 354 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300077 ER PT B AU Nichols, J Mendygral, P AF Nichols, J. Mendygral, P. BE Sonneborn, G Moos, HW Andersson, BG TI FUSE analysis of the Cyg OBI superbubble SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria AB FUSE observations of four stars in the line of sight to the Cyg OB1 IR-detected superbubble have been analyzed for high-velocity features in the O VI interstellar lines, which might be attributed to the shock structure of the superbubble. Multiple components were detected in the spectra of all four stars, with a velocity range of -85 km/s to +29 km/s. As many as four separate velocity components were identified in each spectrum, implying multiple shock structures in the superbubble. Derived column densities of the 0 VI components indicate shock velocities of 160-190 km/s according to steady state shock theory. C1 [Nichols, J.; Mendygral, P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Nichols, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jnichols@cfa.harvard.edu FU NASA [NAG-12612] FX We acknowledge the support of NASA Grant NAG-12612. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 451 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300102 ER PT B AU Szabo, GM Furesz, G Szekely, P Szentgyorgyi, A AF Szabo, Gy. M. Furesz, G. Szekely, P. Szentgyorgyi, A. BE Sterken, C Aerts, C TI Kinematics and variable stars in NGC 1907 and NGC 1912 SO ASTROPHYSICS OF VARIABLE STARS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Astrophysics of Variable Stars CY SEP 05-10, 2005 CL Pecs, HUNGARY AB We introduce our ongoing photometric and spectroscopic survey in the region of open clusters NGC 1907 and NGC 1912. The radial velocity dispersion of about 4 km s(-1) in the clusters supports the interpretationj of physical interaction between them. We found 17 variable stars in the examined fields covering about 2/3 of the "cluster areas'. The relative low number (0.2%) of eclipsing variables supports the broadened internal velocity distribution to be the reason of the increased dispersion. C1 [Szabo, Gy. M.; Szekely, P.] Univ Szeged, Dept Exp Phys & Astron Obs, Dom Ter 9, H-6720 Szeged, Hungary. [Furesz, G.; Szentgyorgyi, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Szabo, GM (reprint author), Univ Szeged, Dept Exp Phys & Astron Obs, Dom Ter 9, H-6720 Szeged, Hungary. EM SZGY@TITAN.PHYSX.U-SZEGED.HU RI Szabo, Gyula/A-8310-2012 FU Hungarian OTKA [T042509] FX This study was supported by the Hungarian OTKA Grant T042509. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-217-2 J9 ASTR SOC P PY 2006 VL 349 BP 339 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEJ62 UT WOS:000237451200051 ER PT J AU Helgen, KM Wells, RT Kear, BP Gerdtz, WR Flannery, TF AF Helgen, Kristofer M. Wells, Rod T. Kear, Benjamin P. Gerdtz, Wayne R. Flannery, Timothy F. TI Ecological and evolutionary significance of sizes of giant extinct kangaroos SO AUSTRALIAN JOURNAL OF ZOOLOGY LA English DT Article ID PLEISTOCENE MARSUPIAL LION; BODY-SIZE; MAMMALS; MASS; ALLOMETRY; AUSTRALIA; MEGAFAUNA; DINOSAURS; WEIGHT; FAUNAS AB A method, based on femoral circumference, allowed us to develop body mass estimates for 11 extinct Pleistocene megafaunal species of macropodids (Protemnodon anak, P. brehus, P. hopei, P. roechus, Procoptodon goliah, 'P.' gilli, Simosthenurus maddocki, S. occidentalis, Sthenurus andersoni, S. stirlingi and S. tindalei) and three fossil populations of the extant eastern grey kangaroo ( Macropus giganteus). With the possible exception of P. goliah, the extinct taxa were browsers, among which sympatric, congeneric species sort into size classes separated by body mass increments of 20 - 75%. None show evidence of size variation through time, and only the smallest ('P.' gilli) exhibits evidence suggestive of marked sexual dimorphism. The largest surviving macropodids ( five species of Macropus) are grazers which, although sympatric, do not differ greatly in body mass today, but at least one species ( M. giganteus) fluctuated markedly in body size over the course of the Pleistocene. Sexual dimorphism in these species is marked, and may have varied through time. There is some mass overlap between the extinct and surviving macropodid taxa. With a mean estimated body mass of 232 kg, Procoptodon goliah was the largest hopping mammal ever to exist. C1 S Australian Museum, Adelaide, SA 5000, Australia. Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. Deakin Univ, Sch Ecol & Environm, Burwood, Vic 3125, Australia. RP Flannery, TF (reprint author), S Australian Museum, North Terrace, Adelaide, SA 5000, Australia. EM flannery.tim@saugov.sa.gov.au NR 56 TC 18 Z9 18 U1 0 U2 25 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0004-959X J9 AUST J ZOOL JI Aust. J. Zool. PY 2006 VL 54 IS 4 BP 293 EP 303 DI 10.1071/ZO05077 PG 11 WC Zoology SC Zoology GA 072GJ UT WOS:000239661600008 ER PT J AU van Dyk, DA Connors, A Esch, DN Freeman, P Kang, H Karovska, M Kashyap, V Siemiginowska, A Zezas, A AF van Dyk, David A. Connors, Alanna Esch, David N. Freeman, Peter Kang, Hosung Karovska, Margarita Kashyap, Vinay Siemiginowska, Aneta Zezas, Andreas TI Deconvolution in High-Energy Astrophysics: Science, Instrumentation, and Methods SO BAYESIAN ANALYSIS LA English DT Article DE Background ontamination; Censoring; Chandra X-ray Observatory; Chi Square Fitting; Count Data; Contingency Tables; Deconvolution; Differential Emission Measure; EM-type Algorithms; Frequency Evaluations; Richardson-Lucy; Hardness Ratios; Hubble Space Telescope; Image Analysis; Log-Linear Models; Markov chain Monte Carlo; Measurement Errors; Multiscale Methods; Sampling Distributions; Smoothing; Prior Distribution; Point Spread Function; Posterior Predictive Checks; Power Law; Poisson Models; Spectral Analysis; Timing Analysis AB In recent years, there has been an avalanche of new data in observational high-energy astrophysics. Recently launched or soon-to-be launched space-based telescopes that are designed to detect and map ultra-violet, X-ray, and gamma-ray electromagnetic emission are opening a whole new window to study the cosmos. Because the production of high-energy electromagnetic emission requires temperatures of millions of degrees and is an indication of the release of vast quantities of stored energy, these instruments give a completely new perspective on the hot and turbulent regions of the universe. The new instrumentation allows for very high resolution imaging, spectral analysis, and time series analysis; the Chandra X-ray Observatory, for example, produces images atleast thirty times sharper than any previous X-ray telescope. The complexity of the instruments, of the astronomical sources, and of the scientific questions leads to a subtle inference problem that requires sophisticated statistical tools. For example, data are subject to non-uniform stochastic censoring, heteroscedastic errors in measurement, and background contamination. Astronomical sources exhibit complex and irregular spatial structure. Scientists wish to draw conclusions as to the physical environment and structure of the source, the processes and laws which govern the birth and death of planets, stars, and galaxies, and ultimately the structure and evolution of the universe. The California-Harvard Astrostatistics Collaboration is a group of astrophysicists and statisticians working together to develop statistical methods, computational techniques, and freely available software to address outstanding inferential problems in high-energy astrophysics. We emphasize fully model-based statistical inference; we explicitly model the complexities of both astronomical sources and the data generation mechanisms inherent in new high-tech instruments, and fully utilize the resulting highly structured models in learning about the underlying astronomical and physical processes. Using these models requires sophisticated scientific computation, advanced methods for statistical inference, and careful model checking procedures. Here we discuss the broad scientific goals of observation high-energy astrophysics, the specifics of the data collection mechanism involved with the Chandra X-ray Observatory, current statistical methods, and the Bayesian models and methods that we propose. We illustrate our statistical strategy in the context of several applied examples, including the estimation of hardness ratios, spectral analysis, multiscale image analysis, and reconstruction of the distribution of the temperature of hot plasma in a stellar corona. This paper was presented at the Case Studies in Bayesian Statistics Workshop 7 held at Carnegie Mellon University in September 2003. C1 [van Dyk, David A.] Univ Calif Irvine, Dept Stat, Irvine, CA 92717 USA. [Connors, Alanna] Eureka Sci, Oakland, CA USA. [Esch, David N.; Kang, Hosung] Harvard Univ, Dept Stat, Boston, MA 02115 USA. [Freeman, Peter; Karovska, Margarita; Kashyap, Vinay; Siemiginowska, Aneta; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Boston, MA USA. RP van Dyk, DA (reprint author), Univ Calif Irvine, Dept Stat, Irvine, CA 92717 USA. EM pfreeman@cmu.edu; mkarovska@cfa.harvard.edu; azezas@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 68 TC 5 Z9 5 U1 0 U2 2 PU INT SOC BAYESIAN ANALYSIS PI PITTSBURGH PA CARNEGIE MELLON UNIV, DEPT STTISTICS, PITTSBURGH, PA 15213 USA SN 1931-6690 J9 BAYESIAN ANAL JI Bayesian Anal. PY 2006 VL 1 IS 2 BP 189 EP 235 PG 47 WC Mathematics, Interdisciplinary Applications; Statistics & Probability SC Mathematics GA V10EI UT WOS:000207446900001 ER PT J AU Kelber, A Warrant, EJ Pfaff, M Wallen, R Theobald, JC Wcislo, WT Raguso, RA AF Kelber, A Warrant, EJ Pfaff, M Wallen, R Theobald, JC Wcislo, WT Raguso, RA TI Light intensity limits foraging activity in nocturnal and crepuscular bees SO BEHAVIORAL ECOLOGY LA English DT Article DE bees; eyes; foraging; insects; ocelli; sensitivity; visual ecology ID MEGALOPTA-GENALIS; NEURAL ORGANIZATION; HALICTID BEE; HYMENOPTERA; APOIDEA; BEHAVIOR; ORIENTATION; POLLINATION; PHENOLOGY; PATTERNS AB A crepuscular or nocturnal lifestyle has evolved in bees several times independently, probably to explore rewarding pollen sources without competition and to minimize predation and nest parasites. Despite these obvious advantages, only few bee species are nocturnal. Here we show that the sensitivity of the bee apposition eye is a major factor limiting the ability to forage in dim light. We present data on eye size, foraging times, and light levels for Megalopta genalis (Augochlorini, Halictidae) in Panama, and Lasioglossum (Sphecodogastra) sp. (Halictini, Halictidae) in Utah, USA. M. genalis females forage exclusively during twilight, but as a result of dim light levels in the rain forest, they are adapted to extremely low intensities. The likely factor limiting their foraging activity is finding their nest entrance on return from a foraging trip. The lowest light intensity at which they can do this, both in the morning and the evening, is 0.0001 cd m(-2). Therefore, they leave the nest at dimmer light levels in the morning than in the evening. Lasioglossum (Sphecodogastra) foraging is limited by light intensity in the evening, but probably by temperature in the morning in the temperate climate of Utah. We propose that the evolution of nocturnality in bees was favored by the large variance in the size of females. C1 Lund Univ, Dept Cell & Organism Biol Zool, S-22362 Lund, Sweden. Smithsonian Trop Res Inst, Balboa, Panama. Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA. RP Kelber, A (reprint author), Lund Univ, Dept Cell & Organism Biol Zool, Helgonavagen 3, S-22362 Lund, Sweden. EM almut.kelber@cob.lu.se RI Kelber, Almut/H-6216-2014 OI Kelber, Almut/0000-0003-3937-2808 NR 35 TC 72 Z9 73 U1 2 U2 20 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD JAN-FEB PY 2006 VL 17 IS 1 BP 63 EP 72 DI 10.1093/beheco/arj001 PG 10 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 987AD UT WOS:000233489900010 ER PT J AU Eltz, T Roubik, DW Lunau, K AF Eltz, T Roubik, DW Lunau, K TI Experience-dependent choices ensure species-specific fragrance accumulation in male orchid bees (vol 59, pg 149, 2005) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Correction C1 Univ Dusseldorf, Dept Neurobiol, Sensory Ecol Grp, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Eltz, T (reprint author), Univ Dusseldorf, Dept Neurobiol, Sensory Ecol Grp, Univ Str 1, D-40225 Dusseldorf, Germany. EM eltz@uni-duesseldorf.de NR 1 TC 1 Z9 1 U1 0 U2 1 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 JAN PY 2006 VL 59 IS 3 BP 460 EP 460 DI 10.1007/s00265-005-0093-9 PG 1 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 002GW UT WOS:000234600500015 ER PT J AU Piperno, DR AF Piperno, Dolores R. BE Kennett, DJ Winterhalder, B TI The Origins of Plant Cultivation and Domestication in the Neotropics SO BEHAVIORAL ECOLOGY AND THE TRANSITION TO AGRICULTURE SE Origins of Human Behavior and Culture LA English DT Article; Book Chapter AB During the past 20 years, evolutionary biologists have broadened the study of Darwinian processes by drawing on elements from the ecological and behavioral sciences, and asking questions relating to why as well as to how. As a result, flexible decision making by animals, local ecological circumstances, and rapid, phenotypic-level adjustments are viewed as fundamental to evolutionary change. The transition from foraging to farming is, at its heart, an evolutionary transformation, but to avoid a serious paradigm lag with modern biological principles and ensure that our theories can accommodate complex and learned human actions, archaeologists must incorporate these now-standard approaches to adaptive change in biology. This paper uses behavioral ecology, specifically optimal foraging theory (OFT), to examine the origins of plant cultivation and domestication in the American tropics. It reviews the present empirical evidence for early food production in the Neotropical forest, and evaluates four main questions relating to the why and how of agricultural origins, as seen from the perspective of human behavioral ecology (HBE). Using two important genera of American plant domesticates, Cucurbita and Lagenaria, the paper also compares and contrasts the major tenets of HBE with those of other evolutionary programs in archaeology, such as co-evolution, and examines how well the assumptions and predictions of each approach are met by archaeological data. Lastly, it is argued that HBE can be used to explore nomothetic explanations for food production origins because it, alone among the existing generalizing theories, can be applied across cultural and environmental boundaries. C1 [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. [Piperno, Dolores R.] Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. RI Kennett, Douglas/I-7613-2015 OI Kennett, Douglas/0000-0001-5133-9010 NR 0 TC 27 Z9 28 U1 2 U2 4 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93245-6 J9 ORIG HUM BEHAV PY 2006 VL 1 BP 137 EP 166 PG 30 WC Anthropology SC Anthropology GA BWX07 UT WOS:000295177500009 ER PT S AU Honeychurch, W Amartuvshin, C AF Honeychurch, William Amartuvshin, Chunag BE Peterson, DL Popova, LM Smith, AT TI Survey and settlement in Northern Mongolia: The structure of intra-regional nomadic organisation SO Beyond the Steppe and the Sown SE Colloquia Pontifica LA English DT Proceedings Paper CT 1st University-of-Chicago Conference on Eurasian Archeology CY MAY 03-04, 2002 CL Chicago, IL ID HISTORY C1 Smithsonian Inst, Dept Anthropol, NMNH, Washington, DC 20013 USA. NR 47 TC 2 Z9 2 U1 1 U2 3 PU E J BRILL PI PA LEIDEN PA PO BOX 9000, NL-2300 PA LEIDEN, NETHERLANDS SN 1389-8477 BN 90-04-14610-5 J9 COLLOQ PONTICA PY 2006 BP 183 EP 201 PG 19 WC Archaeology SC Archaeology GA BFH62 UT WOS:000241890700010 ER PT J AU Philpott, SM Perfecto, I Vandermeer, J AF Philpott, SM Perfecto, I Vandermeer, J TI Effects of management intensity and season on arboreal ant diversity and abundance in coffee agroecosystems SO BIODIVERSITY AND CONSERVATION LA English DT Article DE agricultural intensification; arboreal ants; biodiversity; Chiapas; coffee agroecosystem; Mexico ID TRAP-NESTING BEES; SPECIES RICHNESS; TROPICAL AGROECOSYSTEM; SHADE COFFEE; BIODIVERSITY CONSERVATION; VEGETATIONAL DIVERSITY; LANDSCAPE CONTEXT; HABITAT FRAGMENTS; NATURAL ENEMIES; SOUTHERN MEXICO AB Agricultural intensification decreases arthropod predator diversity, abundance and population stability, and may affect interactions between top predators and their arthropod prey - ultimately affecting ecosystem services. Coffee management intensification (reduction or removal of shade trees) reduces diversity of arthropod predators (ground-foraging ants). Because ants provide ecosystem services by controlling pests, influences of intensification on arboreal, coffee-foraging ant diversity and abundance are important. We here address how coffee intensification affects: (1) coffee-foraging ant diversity and abundance and (2) seasonal fluctuations in ant abundance. In each of four coffee sites of varying management intensity in Chiapas, Mexico, we sampled vegetation and using two methods, sampled ant diversity and abundance over two years. Sites significantly differed in vegetation and management intensity. Coffee-foraging ant diversity generally decreased with increasing management intensity (16-26% fewer species observed in the most intensively-managed site). Ant abundance was higher in the wet season. Management intensity, however, did not influence ant abundance or seasonal fluctuations in abundance. Our results highlight the importance of diverse agricultural systems in maintaining arthropod predator diversity, and point to one model system in which we may effectively test how diversity per se affects ecosystem services. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. RP Philpott, SM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. EM philpotts@si.edu RI Philpott, Stacy/F-2330-2011 NR 52 TC 42 Z9 47 U1 1 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JAN PY 2006 VL 15 IS 1 BP 139 EP 155 DI 10.1007/s10531-004-4247-2 PG 17 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 022CJ UT WOS:000236032000012 ER PT J AU Philpott, SM Uno, S Maldonado, J AF Philpott, SM Uno, S Maldonado, J TI The importance of ants and high-shade management to coffee pollination and fruit weight in Chiapas, Mexico SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Coffea arabica; ecosystem services; pollinator and ant diversity; shade management system ID SEED SIZE VARIATION; SPECIES RICHNESS; TROPICAL FOREST; EXTRAFLORAL NECTARIES; POLLEN LOAD; HERBIVORE DETERRENCE; PROGENY PERFORMANCE; POLEMONIUM-VISCOSUM; VISITING ANTS; BIODIVERSITY AB Recent reports show importance of pollinators to coffee and importance of ants as pollinators or floral protectors in many systems. Arthropod and pollinator diversity, however, declines with management intensification of coffee (Coffea arabica) agroecosystems. We investigated influences of both flying pollinators and ants on coffee fruit set and fruit weight in one high-shade (high-biodiversity) and one low-shade (low-biodiversity) coffee farm in Chiapas, Mexico through exclusion experiments. Contradictory to previous reports, flying pollinators alone did not affect coffee fruit set or fruit weight. Individual fruit weights, however, were higher on branches with both ants and flying pollinators (1.78 g +/- 0.312 (SE)) compared to branches without ants (1.03 +/- 0.029) or branches without ants or flying pollinators (1.05 +/- 0.049), but only in the high-shade site. Although the mechanisms producing higher fruit weights are unknown, we discuss how ants or ant-flying pollinator interactions under high-shade coffee management may contribute to increased fruit weight and the implications of high-shade management for both sustainable coffee production and biodiversity conservation. C1 Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. El Colegio Frontera Sur, ECOSUR, Tapachula 30700, Chiapas, Mexico. RP Philpott, SM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM philpotts@si.edu RI Philpott, Stacy/F-2330-2011 NR 76 TC 21 Z9 23 U1 5 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JAN PY 2006 VL 15 IS 1 BP 487 EP 501 DI 10.1007/s10531-005-0602-1 PG 15 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 022CJ UT WOS:000236032000032 ER PT J AU Bauer, RA Pelican, KM Pukazhenthi, BS Crosier, AE Ottinger, MA Critser, JK Wildt, DE Howard, J AF Bauer, Rosemary A. Pelican, Katharine M. Pukazhenthi, Budhan S. Crosier, Adrienne E. Ottinger, Mary Ann Critser, John K. Wildt, David E. Howard, JoGayle TI Progestogen priming with altrenogest eliminates spontaneous ovulation and increases sensitivity to exogenous gonadotropins in the cat. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 39th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 29-AUG 01, 2006 CL Univ Nebraska Med Ctr, Omaha, NE SP Soc Study Reprod HO Univ Nebraska Med Ctr C1 Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Univ Maryland, College Pk, MD USA. Univ Missouri, Columbia, MO USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2006 SI SI BP 177 EP 177 PG 1 WC Reproductive Biology SC Reproductive Biology GA 063ZW UT WOS:000239059500525 ER PT J AU Weinbeer, M Meyer, CFJ Kalko, EKV AF Weinbeer, M Meyer, CFJ Kalko, EKV TI Activity pattern of the trawling phyllostomid bat, Macrophyllum macrophyllum, in Panama SO BIOTROPICA LA English DT Article DE Barro Colorado Island; Chiroptera; convergent evolution; foraging behavior; foraging habitat; insectivory; seasonal lowland semideciduous forest; telemetry ID CAROLLIA-PERSPICILLATA CHIROPTERA; FALSE VAMPIRE BAT; FREE-TAILED BATS; FORAGING BEHAVIOR; INSECTIVOROUS BAT; ECHOLOCATION BEHAVIOR; NOCTILIO-LEPORINUS; EUDERMA-MACULATUM; PREDATION RISK; MEGADERMA-LYRA AB We studied activity patterns of long-legged bats, Macrophyllum macrophyllum (Phyllostomidae), in the Barro Colorado Nature Monument, Panama, using radio-telemetry. Activity of four males and five females equipped with radio-transmitters were monitored for 4-7 entire nights each between April and July 2002. Bats exhibited maximum activity around dusk and high activity during the night. Males and females foraged for equal amounts of time in continuous flight (mean: 7 min, maximum 1 h) with interspersed resting phases (mean: 15 min, maximum 3 h). Activity of M. macrophyllum was sensitive to several factors. Time of emergence and return to day roost were correlated with time of sunset and sunrise, respectively. Maximum bat activity coincided with high abundance of aerial insects. Finally, heavy rain caused bats to reduce or cease flight activity. Direct observations and field video recordings support the assumption that M. macrophyllum employs two distinct foraging modes: trawling of insects from and capture of aerial insects at low heights above water. Combination of foraging modes gives M. macrophyllum high flexibility and efficiency in prey search. Activity, foraging mode, and morphology, which are similar to trawling bats from other families, distinguish M. macrophyllum from all other phyllostomid species and grant it access to open habitat above water, a habitat no other phyllostomid bat has conquered. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. RP Kalko, EKV (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. EM elisabeth.kalko@uni-ulm.de RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 NR 55 TC 20 Z9 22 U1 0 U2 12 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 JAN PY 2006 VL 38 IS 1 BP 69 EP 76 DI 10.1111/j.1744-7429.2006.00101.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 005WV UT WOS:000234858000009 ER PT J AU Ruiz-Miranda, CR Affonso, AG de Morais, MM Verona, CE Martins, A Beck, BB AF Ruiz-Miranda, CR Affonso, AG de Morais, MM Verona, CE Martins, A Beck, BB TI Behavioral and ecological interactions between reintroduced golden lion tamarins (Leontopithecus rosalia Linnaeus, 1766) and introduced marmosets (Callithrix spp, Linnaeus, 1758) in Brazil's Atlantic coast forest fragments SO BRAZILIAN ARCHIVES OF BIOLOGY AND TECHNOLOGY LA English DT Article DE ecology; behavior; golden lion tamarin; common marmoset; invasive species; conservation ID NON-INDIGENOUS ORGANISMS; MIXED-SPECIES TROOP; SAGUINUS-FUSCICOLLIS; AMAZONIAN TAMARINS; CALLITRICHIDS; MYSTAX; WILD; BENEFITS; PATTERNS AB Marmosets (Callithrix spp.) have been introduced widely in areas within Rio de Janeiro state assigned for the reintroduction of the endangered golden lion tamarin (Leontopithecus rosalia). The objetives of this study were to estimate the marmoset (CM) population in two fragments with reintroduced golden lion tamarin to quantify the association and characterize the interactions between species. The CM population density (0,09 ind/ha) was higher than that of the golden lion tamarin (0,06 ind/za). The mean association index between tamarins and marmosets varied among groups and seasons (winter=62% and summer=35%). During the winter, competition resulted in increases in territorial and foraging behavior when associated with marmosets. Evidence of benefits during the summer was reduced adult vigilance while associated to marmosets. Golden lion tamarins were also observed feeding on gums obtained from tree gouges made by the marmosets. Marmosets represented a threat for the conservation of golden lion tamarins. C1 Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, BR-28013600 Campos dos Goytacazes, RJ, Brazil. Assoc Mico Leao Dourado, BR-28860970 Casimiro De Abreu, RJ, Brazil. Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. RP Ruiz-Miranda, CR (reprint author), Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, Av Alberto Lamego 2000 Horto, BR-28013600 Campos dos Goytacazes, RJ, Brazil. RI Ruiz-Miranda, Carlos/A-4719-2008; Ruiz-Miranda, Carlos/H-7308-2015; Ruiz, Carlos/I-4446-2016 OI Ruiz-Miranda, Carlos/0000-0001-9786-5315; Ruiz-Miranda, Carlos/0000-0001-7360-0304; NR 53 TC 16 Z9 18 U1 4 U2 31 PU INST TECNOLOGIA PARANA PI CURITIBA-PARANA PA RUA PROF ALGACYR MUNHOZ MADER 3775-CIC, 81350-010 CURITIBA-PARANA, BRAZIL SN 1516-8913 J9 BRAZ ARCH BIOL TECHN JI Braz. Arch. Biol. Technol. PY 2006 VL 49 IS 1 BP 99 EP 109 DI 10.1590/S1516-89132006000100012 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 018QF UT WOS:000235779200012 ER PT J AU Nino, SM Clark, LG Dorr, LJ AF Nino, SM Clark, LG Dorr, LJ TI A new species of Chusquea (Poaceae : Bambusoideae) in Cordillera de Merida, Venezuela SO BRITTONIA LA Spanish DT Article AB A new species of woody bamboo (Poaceae: Bambusoideae). Chusquea guirigayensis, is described and illustrated. This species is placed in Chusquea sect. Swallenochloa (McClure) L. G. Clark because of its shrubby habit. short waxy internodes, intravaginal branching, and linearly arranged subsidiary buds/branches. In addition. we discuss related species, and describe the ecology and distribution of the new species. Separate keys based on sterile and fertile material of the Venezuelan species of C sect. Swalenochloa are provided. C1 Iowa State Univ, Dept EEOB, Ames, IA 50011 USA. Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. EM smiguel@cantv.net; lgclark@iastate.edu; dorrl@si.edu NR 2 TC 1 Z9 2 U1 0 U2 1 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JAN-MAR PY 2006 VL 58 IS 1 BP 46 EP 51 PG 6 WC Plant Sciences SC Plant Sciences GA 033SJ UT WOS:000236869200005 ER PT J AU Lutz, RA Collins, AG Annis, ER Reed, AJ Bennett, KF Halanych, KM Vrijenhoek, RC AF Lutz, Richard A. Collins, Allen G. Annis, Eric R. Reed, Andrew J. Bennett, Kyle F. Halanych, Kenneth M. Vrijenhoek, Robert C. TI Stauromedusan populations inhabiting deep-sea hydrothermal vents along the southern East Pacific Rise SO CAHIERS DE BIOLOGIE MARINE LA English DT Article; Proceedings Paper CT 3rd International Symposium on Hydrothermal Vent and Seep Biology CY SEP 12-16, 2006 CL La Jolla, CA SP Natl Sci Fdn, Ridge 2000 Program, Scripps Inst Oceanog, Census Marine Life, NOAA Undersea Res Program, Minerals Management Serv, NOAAs Off Ocean Explorat, InterRidge, New EnglandBiolabs DE stauromedusae; Lucernaria; hydrothermal vents; East Pacific Rise; 16S sequences ID PHYLOGENY; CNIDARIA AB Dense populations of "stalked jellyfish" (Stauromedusae) were encountered at two geographically-separated, deep-sea hydrothermal vent fields located at 7 degrees 26'S; and 20 degrees 02'S along the East Pacific Rise (EPR). DSV Alvin was utilized (on dives 3320 and 3334) at the sites to collect numerous stauromedusans, which were immediately frozen (at -70 degrees C) or preserved in 70% ethanol upon arrival on board the research support vessel (R/V Atlantis). High resolution images were collected of the organisms in situ. A 530-560-bp region of mitochondrial 16S was amplified, and edited 16S sequences were aligned, along with sequences from 7 other stauromedusans. Results suggest that the Stauromedusae encountered at 7 degrees 26'S, and 20 degrees 02'S are very closely related, if not conspecific. It remains unclear whether or not these Stauromedusae are distinct from Lucernaria janetae (collected from 8 degrees 37'N along the EPR), which was recently described by Collins and Daly (2005). To date, dense populations of stauromedusans have been encountered at four separate deep-sea hydrothermal vent fields along the EPR located at the following latitudes: 20 degrees 50'N, 8 degrees 37'N, 7 degrees 26'S and 20 degrees 02'S. Many fascinating questions remain concerning the biogeography and mechanisms of dispersal of these cnidarians between discrete deep-sea hydrothermal systems. C1 Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. Smithsonian Inst, NOAAs Fisheries Serv, Natl Museum Nat Hist, Natl Systemat Lab, Washington, DC 20013 USA. Auburn Univ, Dept Life Sci, Auburn, AL 36849 USA. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Lutz, RA (reprint author), Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. EM rlutz@imcs.rutgers.edu RI Collins, Allen/A-7944-2008; Halanych, Ken/A-9480-2009 OI Collins, Allen/0000-0002-3664-9691; Halanych, Ken/0000-0002-8658-9674 NR 12 TC 4 Z9 4 U1 0 U2 6 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2006 VL 47 IS 4 BP 409 EP 413 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 129SV UT WOS:000243751300013 ER PT J AU Kitchen, AM Gese, EM Lupis, SG AF Kitchen, Ann M. Gese, Eric M. Lupis, Sarah G. TI Multiple scale den site selection by Swift Foxes, Vulpes velox, in southeastern Colorado SO CANADIAN FIELD-NATURALIST LA English DT Article DE Swift Fox; Vulpes velox; denning; habitat selection; home range use; Colorado ID HOME-RANGE; HABITAT USE; COYOTES; DIET; ECOLOGY AB Predation by Coyotes (Canis latrans) is a major source of mortality in Swift Fox (Vulpes velox) populations. Year-round den use by Swift Foxes is likely to be a predator avoidance strategy. Due to the importance of denning to Swift Fox ecology, we recorded den site selection of Swift Foxes in southeastern Colorado. Den site selection was recorded at two scales: microhabitat characteristics at the den and den placement within the home range. The number of den entrances, height and width of each entrance, aspect, hill position, slope, percent rock in soil, vegetative cover, and horizontal foliar density of 42 Swift Fox dens were examined during December 1999 -April 2000. This was compared to the same microhabitat characteristics at 42 random sites within Swift Fox home ranges to determine if Swift Foxes were using site characteristics according to their availability. Our results indicated that Swift Foxes were not highly selective of den sites based on the microhabitat characteristics evaluated in this study, although Swift Foxes selected areas of intermediate rock percentages. In addition, Swift Foxes were radio-tracked throughout the sample period and the location and frequency of use of known dens were recorded. Within the core area of home ranges, Swift Foxes used more dens (mean = 3.51 +/- 1.70 (SD)), and had a higher frequency of use of dens (mean = 8.20 +/- 6.01) than in the mid-range area (number of dens, mean = 0.90 +/- 0.94; frequency, mean = 1.27 +/- 2.12) and the boundary area (number of dens, mean = 0.34 +/- 0.53; frequency, mean = 0.45 +/- 0.93) of the home range. We discuss our results in terms of the importance of dens in facilitating escape from Coyotes. These results illustrate the need for examining den site selection at multiple scales to determine all selection factors, and to provide information useful for recovery and management efforts for this species. C1 Utah State Univ, Dept Forest Range & Wildlife Sci, Natl Wildlife Res Ctr, USDA,Wildlife Serv, Logan, UT 84322 USA. RP Kitchen, AM (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20013 USA. EM HendersonAn@si.edu RI Gese, Eric/B-4578-2011 NR 35 TC 2 Z9 2 U1 0 U2 15 PU OTTAWA FIELD-NATURALISTS CLUB PI OTTAWA PA PO BOX 35069, WESTGATE PO, OTTAWA, ONTARIO K1Z 1A2, CANADA SN 0008-3550 J9 CAN FIELD NAT JI Can. Field-Nat. PD JAN-MAR PY 2006 VL 120 IS 1 BP 31 EP 38 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 190OD UT WOS:000248067600006 ER PT J AU Fulford, RS Rice, JA Miller, TJ Binkowski, FP AF Fulford, RS Rice, JA Miller, TJ Binkowski, FP TI Elucidating patterns of size-dependent predation on larval yellow perch (Perca flavescens) in Lake Michigan: an experimental and modeling approach SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID INDIVIDUAL-BASED MODEL; RECRUITMENT MECHANISMS; ALOSA-PSEUDOHARENGUS; CLUPEA-HARENGUS; MARINE FISHES; EARLY-LIFE; BODY-SIZE; PREY; SURVIVAL; ALEWIFE AB Yellow perch (Perca flavescens) in Lake Michigan have experienced sustained recruitment failure since 1990 as a result of increased mortality during the pelagic larval phase. Increased mortality of larval yellow perch has been tied indirectly to increased alewife (Alosa pseudoharengus) predation, but effects of predation on larval survival variability must be better understood. We compared the relative importance of predation by alewife and two other fish predators to larval survival in laboratory experiments and developed an individual-based predation model (IBM) to examine patterns in size-dependent predation vulnerability. Simulations exposing larval perch to predation by all predators suggest that larval mortality resulting from alewife predation is more size-dependent than mortality resulting from the other two predators, and the range of sizes vulnerable to alewife is smaller. Alewife predation may not be an important mortality source for larval yellow perch in Lake Michigan at present because of the narrow range of vulnerable sizes and low densities of larval perch in the open lake. Predation is more likely to be important in smaller, more productive systems where other predators are abundant. Modeling results also indicate IBM analysis of date of hatch distributions of surviving larvae is a valuable tool for identifying factors most important to larval survival. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. N Carolina State Univ, Dept Zool, Raleigh, NC 27695 USA. Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. Great Lakes WATER Inst, Milwaukee, WI 53204 USA. RP Fulford, RS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM fulfordr@si.edu RI Miller, Thomas/C-2129-2008 OI Miller, Thomas/0000-0001-8427-1614 NR 50 TC 9 Z9 9 U1 2 U2 8 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JAN PY 2006 VL 63 IS 1 BP 11 EP 27 DI 10.1139/F05-195 PG 17 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 010XO UT WOS:000235231400002 ER PT J AU Fulford, RS Rice, JA Miller, TJ Binkowski, FP Dettmers, JM Belonger, B AF Fulford, RS Rice, JA Miller, TJ Binkowski, FP Dettmers, JM Belonger, B TI Foraging selectivity by larval yellow perch (Perca flavescens): implications for understanding recruitment in small and large lakes SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID MUSSELS DREISSENA-POLYMORPHA; PREY SELECTION; ONEIDA-LAKE; NEW-YORK; BEHAVIORAL MECHANISMS; PLANKTIVOROUS FISH; GAPE LIMITATION; VISUAL-ACUITY; YOUNG; ZOOPLANKTON AB Growth and survivorship of larval yellow perch (Perca flavescens) have been examined in many systems but can conclusions from well-studied perch populations in smaller lakes be applied to populations in meso-oceanic systems like Lake Michigan, USA? Laboratory experiments were conducted with yellow perch (hatch to 35 mm total length) to develop an empirical selectivity function based on Chesson's alpha to describe larval diet as a function of changes in prey community composition. This function was used in an individual-based foraging and growth model (IBM) to describe changes in foraging decisions resulting from changes in prey composition between different systems. Larval perch made three selective transitions during ontogeny. Initial positive selection for rotifers and the relative selectivity for cladocerans vs. copepods in late-stage larvae were both dependent on prey composition. Larvae exposed to prey assemblages differing only in composition had different diets. The empirically based IBM accurately predicted these dietary differences and resulting differences in larval growth and likelihood of starvation between systems at equal prey density. The importance of feeding behavior to larval survival will differ between Lake Michigan and smaller lakes, and these results are important for comparisons of recruitment dynamics between large and small systems. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. N Carolina State Univ, Dept Zool, Raleigh, NC 27695 USA. Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. Great LAKES Water Inst, Milwaukee, WI 53204 USA. Illinois Nat Hist Survey, Lake Michigan Biol Stn, Zion, IL 60099 USA. Wisconsin Dept Nat Resources, Peshtigo, WI 54157 USA. RP Fulford, RS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM fulfordr@si.edu RI Miller, Thomas/C-2129-2008 OI Miller, Thomas/0000-0001-8427-1614 NR 49 TC 26 Z9 28 U1 1 U2 32 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD JAN PY 2006 VL 63 IS 1 BP 28 EP 42 DI 10.1139/F05-196 PG 15 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 010XO UT WOS:000235231400003 ER PT S AU Lorenzini, EC Shapiro, II Ashenberg, J Bombardelli, C Cheimets, PN Iafolla, V Lucchesi, DM Nozzili, S Santoli, F Glashow, S AF Lorenzini, E. C. Shapiro, I. I. Ashenberg, J. Bombardelli, C. Cheimets, P. N. Iafolla, V. Lucchesi, D. M. Nozzili, S. Santoli, F. Glashow, S. BE Mornas, L Alonso, JD TI Detector configurations for equivalence principle tests with strong separation of signal from noise SO CENTURY OF RELATIVITY PHYSICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 28th Spanish Relativity Meeting CY SEP 06-10, 2005 CL Oviedo, SPAIN SP Univ Oviedo, Phys Dept, Spanish Soc Gravitat & Relativ, Prince Felipe Auditorium, Municipal Oviedo, CajAstur, Spanish Embassy Cuba, Spanish Agcy Int Cooperat, European Phys Soc, E W Task Force Program DE experimental tests of gravitational theories; mechanical instruments; design of experiments; computer modeling and simulation; Equivalence Principle ID MISSION AB Testing the Equivalence Principle (EP) at a level of accuracy substantially higher than the present state of the art requires resolving a very small signal out of the instrument's intrinsic noise and also the noise associated with the instrument's motion and gravity gradients. In the test of the Equivalence Principle in an Einstein Elevator under development by our team, the acceleration detector spins about a horizontal axis while free failing for about 25 s inside a co-moving capsule released from a stratospheric balloon. The characteristics of the instrument package and the configuration of the detector play a key role in the ability to extract an EP violation signal at the desired threshold level out of dynamics-related noise. Numerical simulations of the detector's dynamics in the presence of relevant perturbations, having assumed realistic errors and construction imperfections, show the merits of the detector configuration selected. The results illustrate that the effects of dynamics and gravity gradients, near or at the signal frequency, can be limited to levels much smaller than the expected threshold sensitivity of the detector. C1 [Lorenzini, E. C.; Shapiro, I. I.; Ashenberg, J.; Bombardelli, C.; Cheimets, P. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Iafolla, V.; Lucchesi, D. M.; Nozzili, S.; Santoli, F.] Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Glashow, S.] Boston Univ, Boston, MA 02215 USA. RP Lorenzini, EC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elorenzini@cfa.harvard.edu; iafolla@ifsi.rm.cnr.it OI Santoli, Francesco/0000-0003-2493-0109 FU NASA Glenn [NAG3-2881]; Smithsonian Astrophysical Observatory; Italian Space Agency [I/R/098/02]; Institute of Interplanetary Space Physics FX The authors would like to acknowledge the financial support from NASA Glenn through Grant NAG3-2881 to the Smithsonian Astrophysical Observatory and from the Italian Space Agency through contract I/R/098/02 to the Institute of Interplanetary Space Physics. NR 8 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0333-3 J9 AIP CONF PROC PY 2006 VL 841 BP 502 EP + PG 2 WC Physics, Multidisciplinary SC Physics GA BET18 UT WOS:000239410700060 ER PT J AU Krot, AN Petaev, MI Keil, K AF Krot, AN Petaev, MI Keil, K TI Mineralogy and petrology of Al-rich objects and amoeboid olivine aggregates in the CH carbonaceous chondrite North West Africa 739 SO CHEMIE DER ERDE-GEOCHEMISTRY LA English DT Article DE Ca, Al-rich inclusions; amoeboid olivine aggregates; Al-rich chondrules; solar nebula; CH carbonaceous chondrites ID REDUCED-CV CHONDRITES; ZONED METAL GRAINS; FERROMAGNESIAN CHONDRULES; REFRACTORY INCLUSIONS; ISOTOPIC COMPOSITIONS; CONDENSATION ORIGIN; GENETIC LINKS; SOLAR NEBULA; CALCIUM; CR AB The aluminum-rich (> 10wt% Al2O3) objects in the CH carbonaceous chondrite North West Africa (NWA) 739 include Ca,Al-rich inclusions (CAIs), Al-rich chondrules, and isolated mineral grains (spinel, plagioclase, glass). Based on the major mineralogy, 54 refractory inclusions found in about 1 cm 2 polished section of NWA 739 can be divided into hibonite-rich (16%), grossite-rich (26%), melilite-rich (28%), spinel-pyroxene-rich (16%) CAIs, and amoeboid olivine aggregates, (AOA's, 17%). Most CAIs are rounded, 25-185 mu m (average = 70 pm) in apparent diameter, contain abundant, tiny perovskite grains, and typically Surrounded by a single- or double-layered rim composed of melilite and/or Al-diopside; occasionally, layers of spinel+hibonite and forsterite are observed. The AOAs are irregularly shaped, 100-250 mu m (average = 175 mu m) in size, and consist of forsterite, Fe,.Ni-metal, and CAIs composed of Al-diopside, anorthite, and minor spinel. One AOA contains compact, rounded melilite-spinel-perovskite CAIs and low-Ca pyroxene replacing forsterite. The Al-rich (> 10 wt% bulk Al2O3) chondrules are divided into Al-diopside-rich and plagioclase-rich. The Al-diopside-rich chondrules. 50-310 mu m (average = 165 mu m) in apparent diameter, consist of Al-diopside, skeletal forsterite, spinel, +/- Al-rich low-Ca pyroxene, and +/- mesostasis. The plagioclase-rich chondrules, 120-455 mu m (average = 285 mu m) in apparent diameter, are composed of low-Ca and high-Ca pyroxenes, forsterite, anorthitic plagioclase, Fe,Ni-metal nodules, and mesostasis. The isolated spinel occurs as coarse, 50-125 mu m in size, subhedral grains, which are probably the fragments of Al-diopside chondrules. The isolated plagioclase grains are too coarse (60-120 mu m) to have been produced by disintegration of chondrules or CAIs; they range in composition from nearly pure anorthite to nearly pure albite; their origin is unclear. The Al-rich objects show no evidence for Fe-alkali metasomatic or aqueous alteration; the only exception is an Al-rich chondrule fragment with anorthite replaced by nepheline. They are texturally and mineralogically similar to those in other CH chondrites studied (Acfer 182, ALH85085, PAT91467, NWA 770), but are distinct from the Al-rich objects in other chondrite groups (CM, CO, CR, CV). The CH CAIs are dominated by very refractory minerals, such as hibonite, grossite, perovskite and gehlenitic melilite, and appear to have experienced very low degrees of high-temperature alteration reactions. These include replacement of grossite by melilite, of melilite by anorthite, diopside, and spinel, and of forsterite by low-Ca pyroxene. Only a few CAIs show evidence for melting and multilayered Wark-Lovering rims. These observations may suggest that CH CAIs experienced rather simple formation history and escaped extensive recycling. In order to preserve the high-temperature mineral assemblages, they must have been efficiently isolated from the hot nebular region, like some chondrules and the zoned Fe,Ni-metal grains in CH chondrites. (c) 2005 Elsevier GmbH. All rights reserved. C1 Univ Hawaii, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. Harvard Univ, Dept Earth & Planetary Sci, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krot, AN (reprint author), Univ Hawaii, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu NR 48 TC 16 Z9 18 U1 1 U2 7 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0009-2819 J9 CHEM ERDE-GEOCHEM JI Chem Erde-Geochem. PY 2006 VL 66 IS 1 BP 57 EP 76 DI 10.1016/j.chemer.2004.03.002 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 029CJ UT WOS:000236535300003 ER PT J AU Grimm, HJ Gilfanov, M Sunyaev, R AF Grimm, Hans-Jakob Gilfanov, Marat Sunyaev, Rashid TI Statistical properties of the combined emission of a discrete source population: Astrophysical implications SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article; Proceedings Paper CT 14th International Carotenoid Symposium CY JUL 20-25, 2005 CL Edinburgh, SCOTLAND DE statistics; X-ray binaries ID X-RAY BINARIES; INDICATOR AB We study the statistical properties of the combined emission of a population of discrete sources. In particular, we consider the dependence of their total luminosity (L-tot = Sigma(k) L-k) and fractional rms(tot) variability on the number of sources n or on the normalization of the luminosity function. We show that due to small number statistics a regime exists, in which L-tot grows non-linearly with n. This is in apparent contradiction with the seemingly obvious prediction < L-tot > = integral LdN/dLdL similar to n. In this non-linear regime, the rmstot decreases with n significantly more slowly than expected from the rms similar to 1/root n averaging law. Only in the limit of n >> I do these quantities behave as intuitively expected, L-tot similar to n and rms(tot) similar to 1 root n. Using the total X-ray luminosity of a galaxy due to its X-ray binary population as an example, we show that the L-X-SFR and L-X-M-* relations predicted from the respective "universal" luminosity functions of high and low mass X-ray binaries are in a good agreement with observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. RP Grimm, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hgrimm@head.cfa.harvard.edu NR 6 TC 5 Z9 5 U1 0 U2 0 PU SCIENCE CHINA PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 SU 1 SI SI BP 197 EP 204 DI 10.1088/1009-9271/6/S1/26 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 138VX UT WOS:000244392500037 ER PT J AU Bao, XM Zhang, HQ Lin, J AF Bao, Xing-Ming Zhang, Hong-Qi Lin, Jun TI Formation of the CME leading edge observed in the 2003 February 18 event SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : flares ID CORONAL MASS EJECTION; SOLAR-FLARES; FILAMENT ERUPTIONS; X-RAY; MORPHOLOGICAL FEATURES; MAGNETIC RECONNECTION; EMERGING FLUX; PROMINENCE; EVOLUTION; MODEL AB This work investigates a typical coronal mass ejection (CME) observed on 2003 February 18, by various space and ground instruments, in white light, H alpha, EUV and X-ray. The H alpha and EUV images indicate that the CME started with the eruption of a long filament located near the solar northwest limb. The white light coronal images show that the CME initiated with the rarefaction of a region above the solar limb and followed by the formation of a bright arcade at the boundary of the rarefying region at height 0.46 R-circle dot above the solar surface. The rarefying process synchronized with the slow rising phase of the eruptive filament, and the CME leading edge was observed to form as the latter started to accelerate. The lower part of the filament brightened in H alpha as the filament rose to a certain height and parts of the filament was visible in the GOES X-ray images during the rise. These brightenings imply that the filament may be heated by the magnetic reconnection below the filament in the early stage of the eruption. We suggest that a possible mechanism which leads to the formation of the CME leading edge and cavity is the magnetic reconnection which takes place below the filament after the filament has reached a certain height. C1 Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bao, XM (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM xbao@bao.ac.cn RI LIN, JUN/B-9890-2017 NR 41 TC 4 Z9 4 U1 0 U2 1 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 IS 6 BP 741 EP 750 DI 10.1088/1009-9271/6/6/14 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 122AM UT WOS:000243198100014 ER PT S AU Faisal, AA Niven, JE AF Faisal, A. Aldo Niven, Jeremy E. BE Berthold, MR Glen, R Fischer, I TI A simple method to simultaneously track the numbers of expressed channel proteins in a neuron SO COMPUTATIONAL LIFE SCIENCES II, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 2nd International Symposium on Computational Life Sciences CY SEP 27-29, 2006 CL Cambridge, ENGLAND SP Mol Graph Modelling Soc, ALTANA Pharma AG, AstraZeneca R&D, Boehringer Ingelheim, Inpharmatica, Unilever R&D Port Sunlight, Unilever Corp Res ID DROSOPHILA PHOTORECEPTORS; K+ CHANNELS; EXCITABILITY; INFORMATION; ENERGY AB Neurons express particular combinations of ion channels that confer specific membrane properties. Although many ion channels have been characterized the functional implications of particular combinations and the regulatory mechanisms controlling their expression are often difficult to assess in vivo and remain unclear. We introduce a method, Reverse Channel Identification (RCI), which enables the numbers and mixture of active ion channels to be determined. We devised a current-clamp stimulus that allows each channels characteristics to be determined. We test our method on simulated data from a computational model of squid giant axons and from fly photoreceptors to identify both the numbers of ion channels and their specific ratios. Our simulations suggest that RCI is a robust method that will allow identification of ion channel number and mixture in vivo. C1 Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. Smithsonian Trop Res Inst, Balboa, Ancon Panama, Panama. RP Faisal, AA (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM a.faisal@zoo.cam.ac.uk RI Faisal, Aldo/A-2367-2009; Niven, Jeremy/A-5883-2011 OI Faisal, Aldo/0000-0003-0813-7207; NR 19 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-45767-4 J9 LECT NOTES COMPUT SC PY 2006 VL 4216 BP 257 EP 267 PG 11 WC Biochemical Research Methods; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Biochemistry & Molecular Biology; Computer Science GA BFI96 UT WOS:000242127600025 ER PT J AU Marquez, A Maldonado, JE Gonzalez, S Beccaceci, MD Garcia, JE Duarte, JMB AF Marquez, Alejandro Maldonado, J. E. Gonzalez, S. Beccaceci, M. D. Garcia, J. E. Duarte, J. M. B. TI Phylogeography and Pleistocene demographic history of the endangered marsh deer (Blastocerus dichotomus) from the Rio de la Plata Basin SO CONSERVATION GENETICS LA English DT Article DE Blastocerus dichotomus; cervidae; conservation; mitochondrial DNA; phylogeography ID POPULATION EXPANSION; PAMPAS DEER; OZOTOCEROS-BEZOARTICUS; CONSERVATION GENETICS; MITOCHONDRIAL-DNA; CLIMATIC CHANGES; CENTRAL BRAZIL; MUTATION-RATE; DIFFERENTIATION; PARAMETERS AB The marsh deer is the largest neotropical cervid with morphological and ecological adaptations to wetlands and riparian habitats. Historically, this now endangered species occupied habitats along the major river basins in South America, ranging from southern Amazonia into northern Argentina to the Parana river delta. This particularly close association with wetlands makes marsh deer an excellent species for studying the effects of Pleistocene climatic changes on their demographic and phylogeographic patterns. We examined mitochondrial DNA variation in 127 marsh deer from 4 areas distributed throughout the Rio de]a Plata basin. We found 17 haplotypes in marsh deer from Brazil, Bolivia and Argentina that differed by 1-8 substitutions in a 601 bp fragment of mitochondrial control region sequence, and 486 bp of cytochrome b revealed only 3 variable sites that defined 4 haplotypes. Phylogeny and distribution of control region haplotypes suggest that populations close to the Pantanal area in central Brazil underwent a rapid population expansion and that this occurred approximately 28,000-25,000 years BP. Paleoclimatic data from this period suggests that there was a dramatic increase for precipitation in the medium latitudes in South America and these conditions may have fostered marsh deer's population growth. C1 IIBCE, Div Citogenet, Unidad Asociada Fac Sci, Montevideo 11600, Uruguay. Smithsonian Inst, Genet Program, Natl Museum Nat Hist, Washington, DC 20008 USA. Univ Salvador, Inst Medio Ambiente & Ecol, Buenos Aires, DF, Argentina. Univ Estadual Londrina, Londrina, SP, Brazil. UNESP, FCAV, Dept Zootecn, BR-14884900 Jaboticabal, SP, Brazil. RP Marquez, A (reprint author), IIBCE, Div Citogenet, Unidad Asociada Fac Sci, Av Italia 3318, Montevideo 11600, Uruguay. EM ale@semic.fcien.edu.uy RI Barbanti Duarte, Jose Mauricio /C-6946-2013 OI Barbanti Duarte, Jose Mauricio /0000-0002-7805-0265 NR 61 TC 15 Z9 18 U1 2 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PY 2006 VL 7 IS 4 BP 563 EP 575 DI 10.1007/s10592-005-9067-8 PG 13 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 086FU UT WOS:000240660000009 ER PT J AU Charola, AE Koestler, RJ AF Charola, A. Elena Koestler, Robert J. BE May, E Jones, M TI Methods in Conservation SO CONSERVATION SCIENCE: HERITAGE MATERIALS LA English DT Article; Book Chapter ID MUSEUM C1 [Charola, A. Elena] World Monuments Fund Portugal, P-1400206 Lisbon, Portugal. [Koestler, Robert J.] Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Charola, AE (reprint author), World Monuments Fund Portugal, P-1400206 Lisbon, Portugal. NR 22 TC 0 Z9 0 U1 0 U2 2 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, CAMBRIDGE CB4 4WF, CAMBS, ENGLAND BN 978-1-84755-762-9 PY 2006 BP 13 EP 31 D2 10.1039/9781847557629 PG 19 WC Art; Chemistry, Multidisciplinary SC Art; Chemistry GA BKZ37 UT WOS:000269680200003 ER PT S AU Knowlton, N AF Knowlton, Nancy BE Cote, IM Reynolds, JD TI Coral reef coda: what can we hope for? SO CORAL REEF CONSERVATION SE Conservation Biology Series LA English DT Article; Book Chapter ID MULTIPLE STABLE STATES; LONG-TERM DECLINE; MARINE RESERVES; HABITAT DESTRUCTION; COUNTRYSIDE BIOGEOGRAPHY; PROTECTED AREAS; CLIMATE-CHANGE; COSTA-RICA; CONSERVATION; BIODIVERSITY C1 [Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat 0202, La Jolla, CA 92093 USA. [Knowlton, Nancy] Smithsonian Trop Res Inst, Balboa, Panama. RP Knowlton, N (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat 0202, La Jolla, CA 92093 USA. NR 47 TC 5 Z9 5 U1 1 U2 16 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1363-3090 BN 978-0-52185-536-5 J9 CONSERV BIOL SER JI Conserv. Biol. Ser. PY 2006 IS 13 BP 538 EP 549 D2 10.2277/ 0521671450 PG 12 WC Biodiversity Conservation; Marine & Freshwater Biology SC Biodiversity & Conservation; Marine & Freshwater Biology GA BYD27 UT WOS:000298093000020 ER PT J AU Kornicker, LS Danielopol, DL Humphreys, WF AF Kornicker, LS Danielopol, DL Humphreys, WF TI Description of the anchialine ostracode, Danielopolina sp cf. D-kornickeri from Christmas Island, Indian Ocean SO CRUSTACEANA LA English DT Article ID EVOLUTION AB The morphology and the systematic affinities of a unique juvenile specimen (post embryonic stage 1) of the ostracode, Danielopolina (family Thaumatocyprididae) are described. It was found in an anchialine cave of Christmas Island, an isolated seamount, and this is the second record of a Danielopolina species in the Indian Ocean. A comparative study of this individual with those belonging to the other 11 Danielopolina species suggests closer morphological affinities to the Australian species, D. kornickeri. In addition, our study allows the separation of the species of Danielopolina into the two new subgenera, Danielopolina and Humphreysella. Tabular keys are provided for the identification of the species belonging to these subgenera. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20013 USA. Austrian Acad Sci, Inst Limnol, A-5310 Mondsee, Austria. Western Australian Museum, Welshpool DC, WA 6986, Australia. RP Kornicker, LS (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20013 USA. EM kornickl@si.edu; Dan.danielopol@oeaw.ac.at; Bill.humphreys@museum.wa.gov.au NR 17 TC 10 Z9 10 U1 1 U2 1 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD JAN PY 2006 VL 79 BP 77 EP 88 DI 10.1163/156854006776759734 PN 1 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 058RE UT WOS:000238681500007 ER PT J AU Lemaitre, R AF Lemaitre, R TI Rectification of events leading to discovery and description of Neoglyphea inopinata Forest & de Saint Laurent, 1975 SO CRUSTACEANA LA English DT Article C1 Museum Natl Hist Nat, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Lemaitre, R (reprint author), Museum Natl Hist Nat, Smithsonian Inst, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM LemaitreR@si.edu NR 1 TC 1 Z9 1 U1 1 U2 1 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD JAN PY 2006 VL 79 BP 123 EP 124 DI 10.1163/156854006776759699 PN 1 PG 2 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 058RE UT WOS:000238681500010 ER PT J AU Zeder, MA Bradley, DG Emshwiller, E Smith, BD AF Zeder, Melinda A. Bradley, Daniel G. Emshwiller, Eve Smith, Bruce D. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Documenting Domestication Bringing Together Plants, Animals, Archaeology, and Genetics SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID MOLECULAR CLOCKS; SUBSTITUTION; AMERICA; MAIZE; RATES; EVOLUTION; REMAINS; ORIGINS; TIMES; DNA C1 [Zeder, Melinda A.; Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. [Bradley, Daniel G.] Trinity Coll Dublin, Smurfit Inst Genet, Dublin, Ireland. [Emshwiller, Eve] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. [Emshwiller, Eve] Univ Wisconsin Madison, Dept Bot, Madison, WI USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RI Emshwiller, Eve/B-9875-2008 OI Emshwiller, Eve/0000-0001-8206-0725 NR 50 TC 5 Z9 5 U1 0 U2 4 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 1 EP 12 PG 12 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200001 ER PT J AU Smith, BD AF Smith, Bruce D. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Documenting Domesticated Plants in the Archaeological Record SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID EVOLUTION; CUCURBITA; PERU; CULTIVATION; SELECTION; VALLEY; MAIZE; LOCUS C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. NR 50 TC 21 Z9 22 U1 1 U2 2 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 15 EP 24 PG 10 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200002 ER PT J AU Smith, BD AF Smith, Bruce D. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Seed Size Increase as a Marker of Domestication in Squash (Cucurbita pepo) SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID EVOLUTION; AMERICA C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. NR 25 TC 10 Z9 11 U1 1 U2 4 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 25 EP 31 PG 7 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200003 ER PT J AU Piperno, DR AF Piperno, Dolores R. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Identifying Manioc (Manihot esculenta Crantz) and Other Crops in Pre-Columbian Tropical America through Starch Grain Analysis A Case Study from Central Panama SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID ETHNOBOTANICAL OBSERVATIONS; COB PHYTOLITHS; CUNA INDIANS; STONE TOOLS; MAIZE; PERU; AGRICULTURE; CULTIVATION; NEOTROPICS; VEGETATION C1 [Piperno, Dolores R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Piperno, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. NR 82 TC 23 Z9 23 U1 1 U2 2 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 46 EP 67 PG 22 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200005 ER PT J AU Zeder, MA AF Zeder, Melinda A. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Archaeological Approaches to Documenting Animal Domestication SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID GOATS CAPRA-HIRCUS; BODY-SIZE; PLEISTOCENE; IRAQ C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. NR 66 TC 17 Z9 18 U1 1 U2 3 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 171 EP 180 PG 10 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200013 ER PT J AU Zeder, MA AF Zeder, Melinda A. BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI A Critical Assessment of Markers of Initial Domestication in Goats (Capra hircus) SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID ANIMAL DOMESTICATION; BONE-STRUCTURE; SHEEP; EAST; IRAQ; AGE C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. NR 86 TC 24 Z9 26 U1 1 U2 6 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 181 EP 208 PG 28 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200014 ER PT J AU Wayne, RK Leonard, JA Vila, C AF Wayne, Robert K. Leonard, Jennifer A. Vila, Carles BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Genetic Analysis of Dog Domestication SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID WOLF CANIS-LUPUS; MITOCHONDRIAL-DNA VARIABILITY; Y-CHROMOSOME; GRAY WOLF; MICROSATELLITE MARKERS; MORPHOLOGICAL CHANGE; ASIAN ORIGIN; ANCIENT DNA; BROWN BEARS; WILD CANIDS C1 [Wayne, Robert K.] Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. [Leonard, Jennifer A.; Vila, Carles] Uppsala Univ, Dept Evolutionary Biol, Uppsala, Sweden. [Leonard, Jennifer A.] Smithsonian Inst, Dept Vertebrate Zool, Genet Program, Washington, DC 20560 USA. [Leonard, Jennifer A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wayne, RK (reprint author), Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. RI Vila, Carles/H-4893-2013; Leonard, Jennifer/A-7894-2010 OI Vila, Carles/0000-0002-4206-5246; Leonard, Jennifer/0000-0003-0291-7819 NR 106 TC 19 Z9 20 U1 0 U2 10 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 279 EP 293 PG 15 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200019 ER PT J AU Vila, C Leonard, JA Beja-Pereira, A AF Vila, Carles Leonard, Jennifer A. Beja-Pereira, Albano BE Zeder, MA Bradley, DG Emshwiller, E Smith, BD TI Genetic Documentation of Horse and Donkey Domestication SO DOCUMENTING DOMESTICATION: NEW GENETIC AND ARCHAEOLOGICAL PARADIGMS LA English DT Article; Book Chapter ID MITOCHONDRIAL-DNA; EQUUS-PRZEWALSKII; ANCIENT DNA; GENUS EQUUS; PHYLOGENETIC-RELATIONSHIPS; MICROSATELLITE DATA; SEQUENCE VARIATION; CHEJU HORSES; ORIGINS; BREEDS C1 [Vila, Carles; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, Uppsala, Sweden. [Leonard, Jennifer A.] Smithsonian Inst, Dept Vertebrate Zool, Sweden Genet Program, Washington, DC 20560 USA. [Leonard, Jennifer A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Beja-Pereira, Albano] Univ Porto, Ctr Invest Biodiversidade & Recursos Genet, Oporto, Portugal. [Beja-Pereira, Albano] Univ Grenoble 1, CNRS, UMR 5553, Lab Biol Populat Altitude, Grenoble, France. RP Vila, C (reprint author), Uppsala Univ, Dept Evolutionary Biol, Uppsala, Sweden. RI Vila, Carles/H-4893-2013; Beja-Pereira, Albano/B-3681-2008; Leonard, Jennifer/A-7894-2010 OI Vila, Carles/0000-0002-4206-5246; Beja-Pereira, Albano/0000-0002-1607-7382; Leonard, Jennifer/0000-0003-0291-7819 NR 86 TC 16 Z9 17 U1 0 U2 6 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-93242-5 PY 2006 BP 342 EP 353 PG 12 WC Archaeology; Evolutionary Biology SC Archaeology; Evolutionary Biology GA BYI78 UT WOS:000298958200024 ER PT J AU Vasquez, CA Nami, HG AF Vasquez, Carlos A. Nami, Hugo G. TI Rock magnetic study of fluvial Holocene soil from Buenos Aires province (Argentina) SO EARTH PLANETS AND SPACE LA English DT Article; Proceedings Paper CT Conference on Paleomagnetism and Tectonics in Latinamerica CY MAY, 2005 CL New Orleans, LA SP AGU DE rock magnetism; Magnetite; Titanomagnetite; Holocene; Buenos Aires ID ENVIRONMENTAL MAGNETISM; LATE PLEISTOCENE; LOESS PLATEAU; RECORD; SEDIMENTS; BULGARIA; PALEOSOL; PLAINS; SIZE AB The magnetic characteristics of soils are widely used in environmental and paleoclimatic investigations for studying the several factors involved in the soil formation process. We propose here a new analytical tool that takes into account the variations in magnetic properties correlated with grain sizes and concentrations of ferrimagnetic minerals. This analytical tool is based on a mathematical model of well-established magnetic properties in samples of known grain sizes and was used in this study to determine changes in the grain size and concentration of ferrimagnetic minerals along a terminal Pleistocene/Holocene fluvial section located in the northeast of Buenos Aires province. These variations may reflect a humid period prevailing in the area and may be associated with climate changes that occurred in the Chaco-Pampean region during the Middle Holocene. C1 Univ Buenos Aires, Ciclo Basico Comun, RA-1428 Buenos Aires, DF, Argentina. Univ Buenos Aires, Fac Ciencias Exactas Fis & Nat, Dept Ciencias Geol, Inst Geofis Daniel A Valencio,CONICET, RA-1428 Buenos Aires, DF, Argentina. Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. RP Vasquez, CA (reprint author), Univ Buenos Aires, Ciclo Basico Comun, Ciudad Univ Pabellon 3, RA-1428 Buenos Aires, DF, Argentina. EM vasquez@gl.fcen.uba.ar NR 50 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 10 BP 1381 EP 1387 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 108XH UT WOS:000242272000017 ER PT J AU Maisch, MW Matzke, AT Brinkmann, W AF Maisch, Michael W. Matzke, Andreas T. Brinkmann, Winand TI The otic capsule of the Middle Triassic ichthyosaur Mixosaurus from Monte San Giorgio (Switzerland): New evidence on the braincase structure of basal ichthyosaurs SO ECLOGAE GEOLOGICAE HELVETIAE LA English DT Article DE Ichthyosauria; Mixosaurus; Braincase; otic capsule; grundplan; Middle Triassic AB For the first time, the otic capsule (prootic and opisthotic) of a Triassic ichthyosaur is described, based on a specimen of Mixosaurus cf. cornalianus from the Grenzbitumenzone of Monte San Giorgio, Switzerland. The otic capsule of Mixosaurus differs from that of more highly derived ichthyosaurs by several features, which are mainly related to the much higher degree of ossification found in Mixosaurus. The prootic is extensively ossified and shows an anteroventral facet for contact with the basisphenoid, a crista prootica lateralis, a foramen completely enclosed by bone for the exit of the nervus facialis, and a posterior sutural contact with the opisthotic, thus closing off the lateral wall of the internal ear capsule. The probtic also forms the anterior margin of a well ossified fenestra vestibuli and has a posterodorsal articulation facet for the supraoccipital. The opisthotic has an elongate, anteroposteriorly compressed, plate-like processus paroccipitalis and shows a well ossified crista interfenestralis, forming the posterior margin of the fenestra vestibuli and the anterior margin of the foramen metoticum. The anterodorsal contact with the supraoccipital is well defined. For all these features, Mixosaurus is much closer to basal amniotes and basal diapsids, such as Captorhinus, Procolophon or Youngina than to more highly derived ichthyosaurs. The new data on the otic capsule of Mixosaurus are corroborated by the braincase of another Middle Triassic ichthyosaur, Phantomovaurits. It can be assumed that the reported features of the Mixosaurus braincase, which are unusual compared with other known ichthyosaurs, could be plesiomorphics retained from an unknown ichthyosaur ancestor, that is representative of the grundplan of ichthyosaurs. However, in the absence of further material the possibility that some features of the mixosaurid otic capsule are autapomorphic within ichthyosaurs can not be excluded. C1 Univ Tubingen, Inst Geowissensch, D-72076 Tubingen, Germany. Smithsonian Inst, NMNH, Dept Paleobiol, NHB MRC 121, Washington, DC 20560 USA. Univ Zurich, Palaontol Inst & Museum, CH-8006 Zurich, Switzerland. RP Maisch, MW (reprint author), Univ Tubingen, Inst Geowissensch, Sigwartstr 1, D-72076 Tubingen, Germany. EM maisch@uni-tuebingen.de; matzke@uni-tuebingen.de; wbrink@pim.unizh.ch NR 29 TC 3 Z9 4 U1 0 U2 2 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0012-9402 J9 ECLOGAE GEOL HELV JI Eclogae Geol. Helv. PY 2006 VL 99 IS 2 BP 205 EP 210 DI 10.1007/s00015-006-1189-6 PG 6 WC Geology SC Geology GA 112YF UT WOS:000242563400005 ER PT J AU Hungate, BA Johnson, DW Dijkstra, P Hymus, G Stiling, P Megonigal, JP Pagel, AL Moan, JL Day, F Li, JH Hinkle, CR Drake, BG AF Hungate, BA Johnson, DW Dijkstra, P Hymus, G Stiling, P Megonigal, JP Pagel, AL Moan, JL Day, F Li, JH Hinkle, CR Drake, BG TI Nitrogen cycling during seven years of atmospheric CO2 enrichment in a scrub oak woodland SO ECOLOGY LA English DT Article DE N-15; nitrogen cycling; progressive nitrogen limitation; rising atmospheric CO2 ID ELEVATED CO2; LONG-TERM; CARBON-DIOXIDE; CALCAREOUS GRASSLAND; FINE ROOTS; ECOSYSTEM; FOREST; RESPONSES; FLORIDA; FIELD AB Experimentally increasing atmospheric CO2 often stimulates plant growth and ecosystem carbon (C) uptake. Biogeochemical theory predicts that these initial responses will immobilize nitrogen (N) in plant biomass and soil organic matter, causing N availability to plants to decline, and reducing the long-term CO2-stimulation of C storage in N limited ecosystems. While many experiments have examined changes in N cycling in response to elevated CO2, empirical tests of this theoretical prediction are scarce. During seven years of postfire recovery in a scrub oak ecosystem, elevated CO2 initially increased plant N accumulation and plant uptake of tracer N-15, peaking after four years of CO2 enrichment. Between years four and seven, these responses to CO2 declined. Elevated CO2 also increased N and tracer N-15 accumulation in the O horizon, and reduced N-15 recovery in underlying mineral soil. These responses are consistent with progressive N limitation: the initial CO2 stimulation of plant growth immobilized N in plant biomass and in the O horizon, progressively reducing N availability to plants. Litterfall production (one measure of aboveground primary productivity) increased initially in response to elevated CO2, but the CO2 stimulation declined during years five through seven, concurrent with the accumulation of N in the O horizon and the apparent restriction of plant N availability. Yet, at the level of aboveground plant biomass (estimated by allometry), progressive N limitation was less apparent, initially because of increased N acquisition from soil and later because of reduced N concentration in biomass as N availability declined. Over this seven-year period, elevated CO2 caused a redistribution of N within the ecosystem, from mineral soils, to plants, to surface organic matter. In N limited ecosystems, such changes in N cycling are likely to reduce the response of plant production to elevated CO2. C1 No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. Univ Nevada, Dept Biol, Reno, NV 89557 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. Kennedy Space Ctr, Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. RP Hungate, BA (reprint author), No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. EM bruce.hungate@nau.edu RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 39 TC 55 Z9 59 U1 1 U2 28 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 JAN PY 2006 VL 87 IS 1 BP 26 EP 40 DI 10.1890/04-1732 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 021XU UT WOS:000236020000005 PM 16634294 ER PT J AU Wright, SJ Calderon, O AF Wright, SJ Calderon, O TI Seasonal, El Nino and longer term changes in flower and seed production in a moist tropical forest SO ECOLOGY LETTERS LA English DT Article DE Barro Colorado Island; El Nino southern oscillation; forest dynamics; La Nina event; lianas; phenology; plant reproduction; solar irradiance; trees ID UNDISTURBED AMAZONIAN FORESTS; SOUTHERN-OSCILLATION; RAIN-FOREST; PERVASIVE ALTERATION; TREE COMMUNITIES; SOLAR-RADIATION; CLIMATE-CHANGE; GROWTH; PHENOLOGY; PATTERNS AB It has recently been reported that humid tropical forests are changing rapidly in response to global anthropogenic change and that these forests experience greater tree mortality and even fire during droughts associated with El Nino events. The former reports are controversial largely because a single method has been used - repeated censuses of tree plots. The latter reports focus on recent extreme El Nino events. Here, we show that flower and seed production both increase during El Nino events in an old-growth tropical forest in Panama. Flower production, but not seed production, has also increased over the past 18 years. The sustained increase in flower production was greater for 33 hana species than for 48 tree species. These results indicate that moderate El Nino events favour seed production, document long-term increases in flower production for the first time, and corroborate long-term increases in the importance of lianas using independent methods. Changes in levels of solar irradiance might contribute to all three patterns. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 53 TC 91 Z9 94 U1 8 U2 51 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD JAN PY 2006 VL 9 IS 1 BP 35 EP 44 DI 10.1111/j.1461-0248.2005.00851.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 011YW UT WOS:000235306400006 PM 16958866 ER PT J AU Dalgarno, A AF Dalgarno, Alexander TI The growth of molecular complexity in the Universe SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemical Evolution of the Universe CY APR 24-26, 2006 CL St Jacut, FRANCE ID POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR CLOUDS; COSMIC-RAY FLUX; EXTRASOLAR PLANET; COMPARATIVE CHEMISTRY; IONIZATION FRACTION; LINE-PROFILES; HOT CORE; RADIATIVE ASSOCIATION; CONTINUUM SOURCES AB A review is presented of the chemistry of the early Universe and the formation of the first stars. The critical role of the formation and destruction of molecular hydrogen in determining their initial mass is demonstrated. A qualitative account is given of the transformation of astrochemistry that occurred in response to the introduction into the Universe of metals. The diagnostic value of astrochemistry is illustrated by its use to infer the Galactic ionization rate. The chemistry of the interstellar medium is contrasted with that of the atmospheres of planets and recent studies of giant extrasolar planets are summarised. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM adalgarno@cfa.harvard.edu NR 172 TC 13 Z9 13 U1 2 U2 10 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 9 EP 25 DI 10.1039/b605715b PG 17 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200001 PM 17191438 ER PT J AU van der Loo, MPJ Groenenboom, GC Jamieson, MJ Dalgarno, A AF van der Loo, Mark P. J. Groenenboom, Gerrit C. Jamieson, Michael J. Dalgarno, Alex TI Raman association of H-2 in the early universe SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemical Evolution of the Universe CY APR 24-26, 2006 CL St Jacut, FRANCE ID DISCRETE VARIABLE REPRESENTATION; HYDROGEN-MOLECULE; TRANSITION MOMENTS; CROSS-SECTIONS; SCATTERING; STATES; POLARIZABILITY; CHEMISTRY; RAYLEIGH; ATOMS AB We investigate the contribution made by Raman scattering to the formation of molecular hydrogen in astrophysical environments characteristic of the early stages of the evolution of the universe. In the Raman process that we study, a photon is scattered by a pair of colliding hydrogen atoms leaving a hydrogen molecule that is stabilized by the transfer of kinetic and binding energy to the photon. We use a formulation for calculating the photon scattering cross section in which an infinite sum of matrix elements over rovibrational levels of dipole accessible electronic states is replaced by a single matrix element of a Green's function. We evaluate this matrix element by using a discrete variable representation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Nijmegen, Inst Theoret Chem, NL-6525 ED Nijmegen, Netherlands. Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. RP van der Loo, MPJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Groenenboom, Gerrit/F-9692-2015; OI Groenenboom, Gerrit/0000-0002-0920-3707 NR 25 TC 1 Z9 1 U1 0 U2 3 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 43 EP 50 DI 10.1039/b516803a PG 8 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200004 PM 17191441 ER PT J AU Buckle, JV Rodgers, SD Wirstrom, ES Charnley, SB Markwick-Kemper, AJ Butner, HM Takakuwa, S AF Buckle, Jane V. Rodgers, Steven D. Wirstrom, Eva S. Charnley, Steven B. Markwick-Kemper, Andrew J. Butner, Harold M. Takakuwa, Shigehisa TI Observations of chemical differentiation in clumpy molecular clouds SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemical Evolution of the Universe CY APR 24-26, 2006 CL St Jacut, FRANCE ID MASS STAR-FORMATION; DISSOCIATIVE RECOMBINATION; DENSE CORES; DARK CLOUD; ORGANIC-MOLECULES; LINE OBSERVATIONS; CHEMISTRY; TMC-1; DEPLETION; SUBMILLIMETER AB We have extensively mapped a sample of dense molecular clouds (L1512, TMC-1C, L1262, Per7, L1389, L1251E) in lines of HC3N, CH3OH, SO and (CO)-O-18. We demonstrate that a high degree of chemical differentiation is present in all of the observed clouds. We analyse the molecular maps for each cloud, demonstrating a systematic chemical differentiation across the sample, which we relate to the evolutionary state of the cloud. We relate our observations to the cloud physical, kinematical and evolutionary properties, and also compare them to the predictions of simple chemical models. The implications of this work for understanding the origin of the clumpy structures and chemical differentiation observed in dense clouds are discussed. C1 Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Natl Astron Observ Japan, ALMA Off, Tokyo 1818588, Japan. RP Buckle, JV (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. EM j.buckle@mrao.cam.ac.uk RI Charnley, Steven/C-9538-2012; OI Butner, Harold/0000-0003-4899-2064; Wirstrom, Eva/0000-0002-0656-876X NR 70 TC 9 Z9 9 U1 1 U2 3 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 63 EP 82 DI 10.1039/b516772h PG 20 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200006 PM 17191443 ER PT J AU Matthews Dalgarno Smith Chakrabarti Black Rawlings Yates Viti Garcia-Burillo van Dishoeck Richards van der Loo Duley Lintott Ehrenfreund Minard Ali Herbst Fuente Plane McCoustra Rowe Ward-Thompson Al-Halabi Geppert Chakrabarti Fraser Schram Palumbo Pilling Buckle Williams Acharyya Yates Semenov AF Matthews Dalgarno Smith Chakrabarti Black Rawlings Yates Viti Garcia-Burillo van Dishoeck Richards van der Loo Duley Lintott Ehrenfreund Minard Ali Herbst Fuente Plane McCoustra Rowe Ward-Thompson Al-Halabi Geppert Chakrabarti Fraser Schram Palumbo Pilling Buckle Williams Acharyya Yates Semenov TI General discussion SO FARADAY DISCUSSIONS LA English DT Editorial Material ID DENSE INTERSTELLAR CLOUDS; UNIMOLECULAR RATE THEORY; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; DISSOCIATIVE CHEMISORPTION; CHEMICAL EVOLUTION; LARGE HYDROCARBONS; MOLECULAR CLOUDS; CARBON CLUSTERS; LINE EMISSION C1 Ctr Space Phys, Kolkata, W Bengal, India. Leiden Univ, NL-2300 RA Leiden, Netherlands. Univ Cambridge, Cambridge CB2 1TN, England. Chalmers, S-41296 Gothenburg, Sweden. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Waterloo, Waterloo, ON N2L 3G1, Canada. Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands. SN Bose Natl Ctr Basic Sci, Kolkata 700064, W Bengal, India. Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. Observ Astron Nacl, Madrid, Spain. UCL, London WC1E 6BT, England. Ohio State Univ, Columbus, OH 43210 USA. Univ Stockholm, Alba Nova, S-10691 Stockholm, Sweden. Jodrell Bank Observ, Macclesfield, Cheshire, England. Penn State Univ, University Pk, PA 16802 USA. Univ Nottingham, Nottingham NG7 2RD, England. Univ Leeds, Leeds LS2 9JT, W Yorkshire, England. Univ Rennes 1, F-35014 Rennes, France. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Eindhoven Univ Technol, NL-5600 MB Eindhoven, Netherlands. Osserv Astrofis Catania, I-95125 Catania, Italy. Cardiff Univ, Cardiff, Wales. Leiden Observ, Leiden, Netherlands. Inst Theoret Chem, Nijmegen, Netherlands. NR 72 TC 0 Z9 0 U1 2 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 83 EP 102 PG 20 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200007 ER PT J AU Sarre Crovisier Kaiser Chakrabarti Richards van Dishoeck Herbst Rowe Semenov Owen Balucani Minard Ehrenfreund Kallenbach Matthews Smith Sims Mitchell Wickham de Bergh Lintott Balucani Herbst Smith Dalgarno Le Picard, Berteloite Canosa Kaiser Black Sarre Pino Rowe Duley Brechignac Pino Cox Biennier Chakrabarti Linnartz AF Sarre Crovisier Kaiser Chakrabarti Richards van Dishoeck Herbst Rowe Semenov Owen Balucani Minard Ehrenfreund Kallenbach Matthews Smith Sims Mitchell Wickham de Bergh Lintott Balucani Herbst Smith Dalgarno Le Picard Berteloite Canosa Kaiser Black Sarre Pino Rowe Duley Brechignac Pino Cox Biennier Chakrabarti Linnartz TI Polycyclic aromatic hydrocarbons, carbon nanoparticles and the diffuse interstellar bands - Discussion SO FARADAY DISCUSSIONS LA English DT Editorial Material ID NEUTRAL FREE-RADICALS; COMET HALE-BOPP; GAS-PHASE; NITROGEN-ATOMS; CROSSED-BEAM; C/1995 O1; ELEMENTARY REACTIONS; TITANS ATMOSPHERE; REACTION CHANNELS; ORGANIC-MATTER C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Rennes 1, F-35014 Rennes, France. Jodrell Bank Observ, Macclesfield, Cheshire, England. Univ Cambridge, Cambridge CB2 1TN, England. Leiden Observ, NL-2300 RA Leiden, Netherlands. Lab Photophys Mol Orsay, Orsay, France. Univ Hawaii, Honolulu, HI 96822 USA. Ohio State Univ, Columbus, OH 43210 USA. Penn State Univ, University Pk, PA 16802 USA. Int Space Sci Inst, Bern, Switzerland. Univ Illinois, Chicago, IL USA. UCL, London WC1E 6BT, England. Observ Paris, F-75014 Paris, France. SN Bose Natl Ctr Basic Sci, Kolkata 700064, W Bengal, India. Univ Perugia, I-06100 Perugia, Italy. Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands. Univ Waterloo, Waterloo, ON N2L 3G1, Canada. Chalmers, S-41296 Gothenburg, Sweden. Univ Manchester, Manchester M13 9PL, Lancs, England. RI Balucani, Nadia/B-8211-2011 OI Balucani, Nadia/0000-0001-5121-5683 NR 84 TC 0 Z9 0 U1 1 U2 3 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 427 EP 448 PG 22 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200028 ER PT J AU Kindlmann, P Kull, T Whigham, D Willems, J AF Kindlmann, P Kull, T Whigham, D Willems, J TI Ecology and population dynamics of terrestrial orchids: An introduction SO FOLIA GEOBOTANICA LA English DT Editorial Material C1 Acad Sci Czech Republ, Inst Syst Biol & Ecol, Dept Theoret Ecol, CZ-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol Sci, CZ-37005 Ceske Budejovice, Czech Republic. Agrocampus Rennes, F-35042 Rennes, France. Estonian Agr Univ, Inst Zool & Bot, EE-51014 Tartu, Estonia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Utrecht, Dept Plant Biol, NL-3508 TB Utrecht, Netherlands. RP Kindlmann, P (reprint author), Acad Sci Czech Republ, Inst Syst Biol & Ecol, Dept Theoret Ecol, Branisovska 31, CZ-37005 Ceske Budejovice, Czech Republic. RI Kindlmann, Pavel/H-7718-2014; Kull, Tiiu/C-5771-2017; OI Kull, Tiiu/0000-0003-2841-7361; Whigham, Dennis/0000-0003-1488-820X NR 4 TC 0 Z9 0 U1 0 U2 7 PU ACAD SCI CZECH REPUBLIC INST BOTANY PI PRAGUE PA PRUHONICE NEAR PRAHA, PRAGUE 252 43, CZECH REPUBLIC SN 1211-9520 J9 FOLIA GEOBOT JI Folia Geobot. PY 2006 VL 41 IS 1 BP 1 EP 2 DI 10.1007/BF02805257 PG 2 WC Plant Sciences SC Plant Sciences GA 008EH UT WOS:000235022500001 ER PT S AU Lee, S Pak, S Geballe, TR Lee, SG Davis, CJ Choi, M Minh, YC Herrnstein, RM Ho, PTP AF Lee, Sungho Pak, Soojong Geballe, T. R. Lee, Sang-Gak Davis, Christopher J. Choi, Minho Minh, Y. C. Herrnstein, Robeson M. Ho, Paul T. P. BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Shock interactions between Sgr A east and its environments SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID GIANT MOLECULAR CLOUDS; GALACTIC-CENTER; MASSIVE STARS; EMISSION; GALAXY; PARSECS; EXPLOSION; SIGNATURE; EVOLUTION; WAVES AB We, have surveyed the interaction regions between Sgr A East and the surrounding molecular clouds in the H-2 1-0 S(l) (2.1218 mu m) line emission. The resulting data cube shows the distribution of the H2 emission both in space (with a resolution of about 2 arcsec) and in velocity (with a resolution of about 18 km s(-1)). Our data are compared with NH3(3,3) data from radio observations to investigate the gas kinematics. Based on the H-2 1 - 0 S(1) line's intensity, its ratio to H-2 2-1 S(1), and its gas kinematics, we conclude that the emitting H-2 is excited by strong molecular shocks. We estimate shock velocities (similar or equal to 100 km s(-1)) by comparing the H2 line profiles with those of NH3, and derive an initial explosion energy of 0.2 - 4 x 10(53) ergs. Such a high energy excludes a single normal supernova for the origin of Sgr A East. We examine other hypotheses, including the tidal disruption of a star by the supermassive black hole (Sgr A*), multiple supernovae, and a hypernova. We suggest that a hypernova, which is believed to originate from a collapsar or microquasar, is the most probable origin. C1 [Lee, Sungho; Choi, Minho; Minh, Y. C.] Korea Astron & Space Inst, 61-1 Hwaam-dong, Taejon 305348, South Korea. [Pak, Soojong] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea. [Geballe, T. R.] Gemini Observ, Hilo, HI 96720 USA. [Lee, Sang-Gak] Seoul Natl Univ, Sch Phys & Astron, Dept Astron, Seoul 151742, South Korea. [Davis, Christopher J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Herrnstein, Robeson M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, S (reprint author), Korea Astron & Space Inst, 61-1 Hwaam-dong, Taejon 305348, South Korea. EM leesh@kasi.re.kr OI Pak, Soojong/0000-0002-2548-238X FU Korean Government; Gemini Observatory FX We thank the staff at UKIRT for their excellent support during our observations. S. Lee thanks Luis Ho for the insightful suggestions on future work. Fig. 1 is reproduced from Fig. 10 of [9] by permission of the AAS. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the U.K. Particle Physics and Astronomy Council. This work was financially supported by the BK21 Project of the Korean Government. T. R. Geballes research is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina,Australia, Brazil, Canada, Chile, the United Kingdom and the United States of America. NR 36 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 22 EP + DI 10.1088/174-6596/54/1/004 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100004 ER PT S AU Montero-Castano, M Herrnstein, RM Ho, PTP AF Montero-Castano, Maria Herrnstein, Robeson M. Ho, Paul T. P. BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Hot molecular gas in the central region around Sgr A SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID GALACTIC-CENTER; CIRCUMNUCLEAR DISK; PARSECS; HCN AB We present our latest Submillimeter Array(1) (SMA) results on HCN(4-3) in the Sgr A* vicinity. We have produced a 37-pointing mosaic, covering a 2' x 2' area around Sgr A*. The angular resolution is 2.5" and the spectral window covered the velocity range of -180 - 1490 km s(-1). We compare our results to the HCN(1-0) observations from the Owens Valley Radio Observatory (OVRO) by [1]. Because of the higher excitation of the (4-3) transition, we find that absorption by lower density foreground material is not important. By comparing the (4-3) and (1-0) results, we find that the excitation is not uniform within the circumnuclear disk (CND). The southern part is stronger in the higher-excitation line. This result was previously suggested by single-dish observations from [2]. We discuss our results in the context of the structure and stability of the CND. C1 [Montero-Castano, Maria; Herrnstein, Robeson M.; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Montero-Castano, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmontero@cfa.harvard.edu FU Academia Sinica Institute of Astronomy and Astrophysics fellowship FX During the development of this study M.M.-C. has been supported by an Academia Sinica Institute of Astronomy and Astrophysics fellowship and a Smithsonian Institution visiting student grant. NR 8 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 29 EP + DI 10.1088/174-6596/54/1/005 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100005 ER PT S AU Marrone, DP Moran, JM Zhao, JH Rao, R AF Marrone, Daniel P. Moran, James M. Zhao, Jun-Hui Rao, Ramprasad BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI The submillimeter polarization of Sgr A* SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; SAGITTARIUS-A; LINEAR-POLARIZATION; GALACTIC-CENTER; X-RAY; CIRCULAR-POLARIZATION; 1 MILLIMETER; RADIO; EMISSION AB We report on the submillimeter properties of Sgr A* derived from observations with the Submillimeter Array and its polarimeter. We find that the spectrum of Sgr A* between 230 and 690 GHz is slightly decreasing when measured simultaneously, indicating a transition to optically thin emission around 300 - 400 GHz. We also present very sensitive and well calibrated measurements of the polarization of Sgr A* at 230 and 345 GHz. With these data we are able to show for the first time that the polarization of Sgr A* varies on hour timescales, as has been observed for the total intensity. On one night we find variability that may arise from a polarized "blob" orbiting the black hole. Finally, we use the ensemble of observations to determine the rotation measure. This represents the first statistically significant rotation measure determination and the only one made without resorting to comparing position angles measured at separate epochs. We find a rotation measure of (-5.6 +/- 0.7) X 10(5) rad m(-2), with no evidence for variability on inter-day timescales at the level of the measurement error. The stability constrains interday fluctuations in the accretion rate to 8%. The mean intrinsic polarization position angle is 167 degrees +/- 7 degrees and we detect variations of 31(-9)(+18) degrees. This separation of intrinsic polarization changes and possible rotation measure fluctuations is now possible because of the frequency coverage and sensitivity of our data. The observable rotation measure restricts the accretion rate to the range 2 x 10(-7) M-circle dot yr(-1) to 2 x 10(-9) M-circle dot yr(-1), if the magnetic field is near equipartition. and ordered. C1 [Marrone, Daniel P.; Moran, James M.; Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rao, Ramprasad] Acad Sinica, Inst Ast & Astrophys, Taipei 10617, Taiwan. RP Marrone, DP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmarrone@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080 NR 41 TC 34 Z9 35 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 354 EP + DI 10.1088/1742-6596/54/1/056 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100056 ER PT S AU Broderick, AE Loeb, A AF Broderick, Avery E. Loeb, Abraham BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Testing general relativity with high-resolution imaging of Sgr A* SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID SUPERMASSIVE BLACK-HOLE; K-ALPHA LINE; GALACTIC-CENTER; ACCRETION DISKS; POLARIZATION; SAGITTARIUS; EMISSION; VARIABILITY; PARAMETERS; RADIATION AB Submilliarcsecond astrometry and imaging of the black hole Sgr A* at the Galactic Center may become possible in the near future at infrared and submillimetre wavelengths. This resolution is sufficient to observe the silhouette the supermassive black hole in the Galactic center casts upon background emission. However, more exciting is the prospect of observing "hot spots" in the accretion flow. Here we discuss how such measurements may be used to test not only the consistency of General Relativity, but also the validity of the Kerr metric in particular. C1 [Broderick, Avery E.; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02145 USA. RP Broderick, AE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02145 USA. EM abroderick@cfa.harvard.edu; aloeb@cfa.harvard.edu FU Harvard College Observatory; NASA [NAG 5-1329, NNG05GH54G]; Clark/Cooke fund of Harvard University FX A.E.B. gratefully acknowledges the support of an ITC Fellowship from Harvard College Observatory. A. L. was supported in part by NASA grants NAG 5-1329 and NNG05GH54G and by the Clark/Cooke fund of Harvard University. NR 33 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 448 EP + DI 10.1088/1742-6596/54/1/070 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100070 ER PT S AU Qin, SL Zhao, JH Moran, JM Marrone, D Patel, N Liu, SY Kuan, YJ Wang, JJ AF Qin, Sheng-Li Zhao, Jun-Hui Moran, James M. Marrone, Daniel Patel, N. Liu, Sheng-Yuan Kuan, Yi-Jehng Wang, Jun-Jie BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Infall, fragmentation, and outflow in Sgr B2 SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID STAR-FORMING REGION; MOLECULAR LINE OBSERVATIONS; SAGITTARIUS B2; HIGH-RESOLUTION; CONTINUUM OBSERVATIONS; FORMALDEHYDE AB Observations of H2CO lines and continuum at 1.3 mm towards Sgr B2(N) and Sgr B2(M) cores were carried out with the SMA. We imaged H2CO line absorption against the continuum cores and the surrounding line emission clumps. The results show that the majority of the dense gas is falling into the major cores where massive stars have been formed. The filaments and clumps of the continuum and gas are detected outside of Sgr B2(N) aud Sgr B2(M) cores. Both the spectra and moment analysis show the presence of outflows from Sgr B2(M) core. The H2CO gas in the red-shifted outflow of Sgr B2(M) appears to be excited by a non-LTE process which might be related to the shocks in the outflow. C1 Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Qin, SL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sqin@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080 NR 16 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 468 EP + DI 10.1088/1742-6596/54/1/073 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100073 ER PT S AU Grindlay, JE AF Grindlay, Jonathan E. CA EXIST Team BE Holt, SS Gehrels, N Nousek, JA TI Post-swift Gamma-ray burst science and capabilities needed to EXIST SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE Gamma-ray bursts; black holes; black hole surveys ID 28 FEBRUARY 1997; DISCOVERY; EMISSION; MISSION AB The exhilerating results from Swift in its first year of operations have opened a new era of exploration of the high energy universe. The surge to higher redshifts of the Gamma-ray bursts now imaged with increased sensitivity establishes them as viable cosmic probes of the early universe. Wide-field coded aperture imaging with solid-state pixel detectors (Cd-Zn-Te) has been also established as the optimum approach for GRB discovery and location as well as to conduct sensitive full-sky hard X-ray sky surveys. I outline the current and future major science questions likely to dominate the post-Swift era for GRBs and several related disciplines and the mission requirements to tackle these. The RUST mission, under study for NASA's Black Hole Finder Probe (BHFP) in the Beyond Einstein Program, could achieve these objectives as the Next Generation GRB Mission with 'ultimate' sensitivity and wide-field survey capability. Analysis tools for processing Swift/BAT slew data are underdevelopment at CfA and will both test DUST scanning imaging and provide new data on GRBs and transients. 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. NR 29 TC 15 Z9 15 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 631 EP 641 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000117 ER PT S AU Sikora, PJ Ogg, JG Gary, A Cervato, C Gradstein, F Huber, BT Marshall, C Stein, JA Wardlaw, B AF Sikora, Paul J. Ogg, James G. Gary, Anthony Cervato, Cinzia Gradstein, Felix Huber, Brian T. Marshall, Charles Stein, Jeffrey A. Wardlaw, Bruce BE Sinha, AK TI An integrated chronostratigraphic data system for the twenty-first century SO GEOINFORMATICS: DATA TO KNOWLEDGE SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE stratigraphy; chronostratigraphy; database; education; research AB Research in stratigraphy is increasingly multidisciplinary and conducted by diverse research teams whose members can be widely separated. This developing distributed-research process, facilitated by the availability of the Internet, promises tremendous future benefits to researchers. However, its full potential is hindered by the absence of a development strategy for the necessary infrastructure. At a National Science Foundation workshop convened in November 2001, thirty quantitative stratigraphers and database specialists from both academia and industry met to discuss how best to integrate their respective chronostratigraphic databases. The main goal was to develop a strategy that would allow efficient distribution and integration of existing data relevant to the study of geologic time. Discussions concentrated on three major themes: database standards and compatibility, strategies and tools for information retrieval and analysis of all types of global and regional stratigraphic data, and future directions for database integration and centralization of currently distributed depositories. The result was a recommendation to establish an integrated chronostratigraphic database, to be called Chronos, which would facilitate greater efficiency in stratigraphic studies (http://www.chronos.org/). The Chronos system will both provide greater ease of data gathering and allow for multidisciplinary synergies, functions of fundamental importance in a variety of research, including time scale construction, paleoenvironmental analysis, paleoclimatology and paleoceanography. Beyond scientific research, Chronos will also provide educational and societal benefits by providing an accessible source of information of general interest (e.g., mass extinctions) and concern (e.g., climatic change). The National Science Foundation has currently funded a three-year program for implementing Chronos. C1 [Sikora, Paul J.; Gary, Anthony] Univ Utah, Energy & Geosci Inst, Salt Lake City, UT 84108 USA. [Ogg, James G.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Cervato, Cinzia] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA 50011 USA. [Gradstein, Felix] Univ Oslo, Museum Geol & Paleontol, N-0562 Oslo, Norway. [Huber, Brian T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Marshall, Charles] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Stein, Jeffrey A.] BP Amer, Houston, TX 77253 USA. [Wardlaw, Bruce] US Geol Survey, Reston, VA 20192 USA. RP Sikora, PJ (reprint author), Univ Utah, Energy & Geosci Inst, 423 Wakara Way,Suite 300, Salt Lake City, UT 84108 USA. EM psikora@egi.utah.edu; jogg@purdue.edu; tgary@egi.utah.edu; cinzia@iastate.edu; felix.gradstein@geolgi.uio.no; huber.brian@nmnh.si.edu; mar-shall@eps.harvard.edu; SteinStop@aol.com; bwardlaw@usgs.gov OI Cervato, Cinzia/0000-0003-4643-1466; Ogg, James/0000-0001-5716-3511 NR 1 TC 1 Z9 1 U1 0 U2 1 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2397-6 J9 GEOL SOC AM SPEC PAP PY 2006 VL 397 BP 53 EP 59 DI 10.1130/2006.2397(04) PG 7 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Geology; Geosciences, Multidisciplinary SC Computer Science; Geology GA BLX56 UT WOS:000271295900005 ER PT J AU Labandeira, CC AF Labandeira, C. C. TI The four phases of plant-arthropod associations in deep time SO GEOLOGICA ACTA LA English DT Review AB Vascular-plant hosts, their arthropod herbivores, and associated functional feeding groups are distributed spatiotemporally into four major herbivore expansions during the past 420 m.y. They are: (1) a Late Silurian to Late Devonian (60 m.y.) phase of myriapod and apterygote, hexapod (perhaps pterygote) herbivores on several clades of primitive vascular-plant hosts and a prototaxalean fungus; (2) a Late Mississippian to end-Permian (85 m.y.) phase of mites and apterygote and basal pterygote herbivores on pteridophyte and basal gymnospermous plant hosts; (3) a Middle Triassic to Recent (245 m.y.) phase of mites, orthopteroids (in the broadest sense) and hernipteroid and basal holometabolan herbivores on pteridophyte and gymnospermous plant hosts; and (4) a mid Early Cretaceous to Recent (115 m.y.) phase of modern-aspect orthopteroids and derived hemipteroid and holometabolous herbivores on angiospermous plant hosts. These host-plant and herbivore associations are mediated by seven functional feeding groups: a) external foliage feeding, b) piercing-and-sucking, c) boring (Phase I origins); d) galling, e) seed predation, f) nonfeeding oviposition (Phase 2 origins); and leaf mining (early Phase 3 origin). Within about 20 m.y. of each herbivore expansion, there is a biota that expresses the nearly full spectrum of later plant-arthropod associations. These four associational phases may be linked to the paleoclimatologic variables of greenhouse/icehouse cycles and atmospheric O-2 and CO2 levels by uncertain causes, although some relationship probably is present. The 7 functional feeding groups persist through most of the sampled interval but harbor host-plants and arthropod herbivores that are spatiotemporally ephemeral. Poor understanding of associations in Phases 1 to 3 is attributed to disproportionate focus on the angiosperm and holometabolan insect associations of Phase 4. RP Labandeira, CC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, POB 37012,MRC-121, Washington, DC 20013 USA. EM labandec@si.edu NR 355 TC 96 Z9 98 U1 3 U2 29 PU UNIV BARCELONA PI BARCELONA PA INST CIENCIES TERRA JAUME ALMERA-CSIC, LLUIS SOLE I SABARIS S-N, BARCELONA, E-08028, SPAIN SN 1695-6133 EI 1696-5728 J9 GEOL ACTA JI Geol. Acta PY 2006 VL 4 IS 4 BP 409 EP 438 PG 30 WC Geology SC Geology GA 128VR UT WOS:000243688300001 ER PT J AU Ellis, S Pan, WS Xie, Z Wildt, DE AF Ellis, Susie Pan, Wenshi Xie, Zhong Wildt, David E. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI The giant panda as a social, biological and conservation phenomenon SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter C1 [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. [Pan, Wenshi] Peking Univ, Coll Life Sci, Beijing 100871, Peoples R China. [Wildt, David E.] Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. [Xie, Zhong] Chinese Assoc Zool Gardens, Beijing 100037, Peoples R China. RP Ellis, S (reprint author), Conservat Int, 1919 M St,Suite 600, Washington, DC 20036 USA. NR 19 TC 9 Z9 9 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 1 EP 16 DI 10.1017/CBO9780511542244.002 D2 10.2277/ 0521832950 PG 16 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600002 ER PT J AU Wildt, DE Zhang, AJ Zhang, HM Xie, Z Janssen, DL Ellis, S AF Wildt, David E. Zhang, Anju Zhang, Hemin Xie, Zhong Janssen, Donald L. Ellis, Susie BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI The Giant Panda Biomedical Survey: how it began and the value of people working together across cultures and disciplines SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID CHEETAH ACINONYX-JUBATUS; NORTH-AMERICAN ZOOS C1 [Wildt, David E.] Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. [Xie, Zhong] Chinese Assoc Zool Gardens, Beijing 100037, Peoples R China. [Zhang, Anju] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [Zhang, Hemin] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Janssen, Donald L.] Zool Soc San Diego, San Diego, CA 92112 USA. [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. RP Wildt, DE (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 8 TC 0 Z9 0 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 17 EP 36 DI 10.1017/CBO9780511542244.003 D2 10.2277/ 0521832950 PG 20 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600003 ER PT J AU Ellis, S Janssen, DL Edwards, MS Howard, J He, GX Yu, JQ Zhang, GQ Wei, RP Miller, RE Wildt, DE AF Ellis, Susie Janssen, Donald L. Edwards, Mark S. Howard, Jogayle He, Guangxin Yu, Jianqiu Zhang, Guiquan Wei, Rongping Miller, R. Eric Wildt, David E. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Factors limiting reproductive success in the giant panda as revealed by a Biomedical Survey SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter C1 [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. [Janssen, Donald L.; Edwards, Mark S.] Zool Soc San Diego, San Diego, CA 92112 USA. [Howard, Jogayle] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [He, Guangxin; Yu, Jianqiu] Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [Zhang, Guiquan; Wei, Rongping] China Res & Conservat Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Miller, R. Eric] WildCare Inst, St Louis Zoo, St Louis, MO 63110 USA. RP Ellis, S (reprint author), Conservat Int, 1919 M St,Suite 600, Washington, DC 20036 USA. NR 8 TC 2 Z9 2 U1 3 U2 10 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 37 EP 58 DI 10.1017/CBO9780511542244.004 D2 10.2277/ 0521832950 PG 22 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600004 ER PT J AU Howard, J Zhang, ZH Li, DS Huang, Y Hou, R Li, GH Zhang, MJ Ye, ZY Zhang, JG Huang, SQ Spindler, RE Zhang, HM Wildt, DE AF Howard, Jogayle Zhang, Zhihe Li, Desheng Huang, Yan Hou, Rong Li, Guanghan Zhang, Meijia Ye, Zhiyong Zhang, Jinguo Huang, Shiqiang Spindler, Rebecca E. Zhang, Hemin Wildt, David E. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Male reproductive biology in giant pandas in breeding programmes in China SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID AILUROPODA-MELANOLEUCA; ZONA-PELLUCIDA; ARTIFICIAL-INSEMINATION; ACROSOMAL INTEGRITY; SPERM CAPACITATION; FLORIDA PANTHERS; SPERMATOZOA; PENETRATION; ELECTROEJACULATION; CRYOPRESERVATION C1 [Howard, Jogayle] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Li, Guanghan] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [Li, Desheng; Huang, Yan; Zhang, Hemin] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Zhang, Jinguo; Huang, Shiqiang] Beijing Zoo, Beijing 100044, Peoples R China. [Spindler, Rebecca E.] Toronto Zoo, Scarborough, ON M1B 5KY, Canada. [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. RP Howard, J (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 38 TC 6 Z9 6 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 159 EP 197 DI 10.1017/CBO9780511542244.008 D2 10.2277/ 0521832950 PG 39 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600008 ER PT J AU Steinman, KJ Monfort, SL McGeehan, L Kersey, DC Gual-Sil, F Snyder, RJ Wang, PY Nakao, T Czekala, NM AF Steinman, Karen J. Monfort, Steven L. McGeehan, Laura Kersey, David C. Gual-Sil, Fernando Snyder, Rebecca J. Wang, Pengyan Nakao, Tatsuko Czekala, Nancy M. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Endocrinology of the giant panda and application of hormone technology to species management SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID AILUROPODA-MELANOLEUCA; DELAYED IMPLANTATION; LUTEINIZING-HORMONE; PROGESTERONE; PREGNANCY; ESTRUS; GONADOTROPINS; TESTOSTERONE; COPULATION; OVULATION C1 [Steinman, Karen J.; Monfort, Steven L.; Kersey, David C.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Czekala, Nancy M.] Zool Soc San Diego, Escondido, CA 92027 USA. [Gual-Sil, Fernando] Zool Chapultepec, Mexico City 11000, DF, Mexico. [McGeehan, Laura] Zool Soc San Diego, Conservat & Res Endangered Species, San Diego, CA 92112 USA. [McGeehan, Laura] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Nakao, Tatsuko] Adventure World, Shirahama, Wakayama 64922, Japan. [Snyder, Rebecca J.] Zoo Atlanta, Atlanta, GA 30315 USA. [Wang, Pengyan] China Res & Conservat Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. RP Steinman, KJ (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 35 TC 17 Z9 17 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 198 EP 230 DI 10.1017/CBO9780511542244.009 D2 10.2277/ 0521832950 PG 33 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600009 ER PT J AU David, VA Sun, S Zhang, ZH Shen, FJ Zhang, GQ Zhang, HM Xie, Z Zhang, YP Ryder, OA Ellis, S Wildt, DE Zhang, AJ O'Brien, SJ AF David, Victor A. Sun, Shan Zhang, Zhihe Shen, Fujun Zhang, Guiquan Zhang, Hemin Xie, Zhong Zhang, Ya-Ping Ryder, Oliver A. Ellis, Susie Wildt, David E. Zhang, Anju O'Brien, Stephen J. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Parentage assessment among captive giant pandas in China SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID AILUROPODA-MELANOLEUCA; CONSERVATION GENETICS; PATERNITY; MICROSATELLITES; POPULATIONS; RELATEDNESS; MARKERS; CUBS C1 [David, Victor A.; Sun, Shan] NCI, Lab Genom Divers, NIH, Frederick, MD 21702 USA. [Shen, Fujun] Chengdu Res Base Giant Panda Breeding, Key Lab Reprod & Conservat Genet, Chengdu 610081, Sichuan Provinc, Peoples R China. [Zhang, Guiquan] China Res & Conservat Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Zhang, Hemin] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Xie, Zhong] Chinese Assoc Zool Gardens, Beijing 100037, Peoples R China. [Zhang, Ya-Ping] Chinese Acad Sci, Key Lab Cellular & Mol Evolut, Kunming Inst Zool, Kunming 650223, Peoples R China. [Ryder, Oliver A.] Zool Soc San Diego, Escondido, CA 92027 USA. [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Zhang, Anju] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [O'Brien, Stephen J.] NCI, Lab Genom Divers, NIH, Frederick, MD 21702 USA. RP David, VA (reprint author), NCI, Lab Genom Divers, NIH, Frederick, MD 21702 USA. NR 34 TC 6 Z9 7 U1 1 U2 4 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 245 EP 273 DI 10.1017/CBO9780511542244.011 D2 10.2277/ 0521832950 PG 29 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600011 ER PT J AU Janssen, DL Morris, P Sutherland-Smith, M Greenberg, M Li, DS Mauroo, N Spelman, L AF Janssen, Donald L. Morris, Patrick Sutherland-Smith, Meg Greenberg, Mark Li, Desheng Mauroo, Nathalie Spelman, Lucy BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Medical management of captive adult and geriatric giant pandas SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID AILUROPODA-MELANOLEUCA C1 [Janssen, Donald L.; Morris, Patrick; Sutherland-Smith, Meg] Zool Soc San Diego, San Diego Zoo, San Diego, CA 92112 USA. [Li, Desheng] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Greenberg, Mark] Univ Calif San Diego, San Diego Med Ctr, San Diego, CA 92103 USA. [Mauroo, Nathalie] Ocean Pk, Aberdeen, Hong Kong, Peoples R China. [Spelman, Lucy] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Janssen, DL (reprint author), Zool Soc San Diego, San Diego Zoo, POB 120551, San Diego, CA 92112 USA. NR 7 TC 6 Z9 6 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 353 EP 376 DI 10.1017/CBO9780511542244.016 D2 10.2277/ 0521832950 PG 24 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600016 ER PT J AU Loeffler, IK Montali, RJ Rideout, BA AF Loeffler, I. Kati Montali, Richard J. Rideout, Bruce A. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Diseases and pathology of giant pandas SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID AILUROPODA-MELANOLEUCA C1 [Loeffler, I. Kati] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Montali, Richard J.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Rideout, Bruce A.] Zool Soc San Diego, San Diego Zoo, San Diego, CA 92112 USA. RP Loeffler, IK (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 32 TC 7 Z9 7 U1 2 U2 10 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 377 EP 409 DI 10.1017/CBO9780511542244.017 D2 10.2277/ 0521832950 PG 33 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600017 ER PT J AU Hildebrandt, TB Brown, JL Goritz, F Ochs, A Morris, P Sutherland-Smith, M AF Hildebrandt, Thomas B. Brown, Janine L. Goeritz, Frank Ochs, Andreas Morris, Patrick Sutherland-Smith, Meg BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Ultrasonography to assess and enhance health and reproduction in the giant panda SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter C1 [Hildebrandt, Thomas B.; Goeritz, Frank] Inst Zoo Biol & Wildlife Res Berlin, D-10315 Berlin, Germany. [Brown, Janine L.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Ochs, Andreas] Zool Garden Berlin AG, D-10787 Berlin, Germany. [Morris, Patrick] Zool Soc San Diego, San Diego Zoo, San Diego, CA 92112 USA. RP Hildebrandt, TB (reprint author), Inst Zoo Biol & Wildlife Res Berlin, Alfred Kowalke Str 17, D-10315 Berlin, Germany. NR 6 TC 1 Z9 2 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 410 EP 439 DI 10.1017/CBO9780511542244.018 D2 10.2277/ 0521832950 PG 30 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600018 ER PT J AU Zhang, ZH Zhang, AJ Hou, R Wang, JS Li, GH Fei, LS Wang, Q Loeffler, IK Wildt, DE Maple, TL McManamon, R Ellis, S AF Zhang, Zhihe Zhang, Anju Hou, Rong Wang, Jishan Li, Guanghan Fei, Lisong Wang, Qiang Loeffler, I. Kati Wildt, David E. Maple, Terry L. McManamon, Rita Ellis, Susie BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Historical perspective of breeding giant pandas ex situ in China and high priorities for the future SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter C1 [Zhang, Zhihe; Zhang, Anju; Li, Guanghan] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [Fei, Lisong; Wang, Qiang] Chengdu Zoo, Chengdu 610081, Sichuan Provinc, Peoples R China. [Loeffler, I. Kati; Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Maple, Terry L.] Georgia Inst Technol, Ctr Conservat & Behav, Sch Psychol, Atlanta, GA 30332 USA. [McManamon, Rita] Zoo Atlanta, Atlanta, GA 30315 USA. [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. RP Zhang, ZH (reprint author), Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, 26 Panda Rd, Chengdu 610081, Sichuan Provinc, Peoples R China. NR 5 TC 11 Z9 11 U1 1 U2 8 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 455 EP 468 DI 10.1017/CBO9780511542244.020 D2 10.2277/ 0521832950 PG 14 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600020 ER PT J AU Howard, J Huang, Y Wang, PY Li, DS Zhang, GQ Hou, R Zhang, ZH Durrant, BS Spindler, RE Zhang, HM Zhang, AJ Wildt, DE AF Howard, Jogayle Huang, Yan Wang, Pengyan Li, Desheng Zhang, Guiquan Hou, Rong Zhang, Zhihe Durrant, Barbara S. Spindler, Rebecca E. Zhang, Hemin Zhang, Anju Wildt, David E. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Role and efficiency of artificial insemination and genome resource banking SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID GIANT PANDA AILUROPODA; MELANOLEUCA; OVULATION; STORAGE; ESTRUS; SPERM C1 [Howard, Jogayle] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Huang, Yan; Li, Desheng; Zhang, Hemin] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Wang, Pengyan; Zhang, Guiquan] China Res & Conservat Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Zhang, Anju] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. [Durrant, Barbara S.] Zool Soc San Diego, Escondido, CA 92027 USA. [Spindler, Rebecca E.] Toronto Zoo, Scarborough, ON M1B 5KY, Canada. [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Howard, J (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 26 TC 11 Z9 11 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 469 EP 494 DI 10.1017/CBO9780511542244.021 D2 10.2277/ 0521832950 PG 26 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600021 ER PT J AU Ballou, JD Miller, PS Xie, Z Wei, RP Zhang, HM Zhang, AJ Huang, SQ Sun, S David, VA O'Brien, SJ Traylor-Holzer, K Seal, US Wildt, DE AF Ballou, Jonathan D. Miller, Philip S. Xie, Zhong Wei, Rongping Zhang, Hemin Zhang, Anju Huang, Shiqiang Sun, Shan David, Victor A. O'Brien, Stephen J. Traylor-Holzer, Kathy Seal, Ulysses S. Wildt, David E. BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Analysis of demographic and genetic trends for developing a captive breeding masterplan for the giant panda SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter ID MAMMALIAN POPULATIONS; MANAGEMENT C1 [Ballou, Jonathan D.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Sun, Shan; David, Victor A.; O'Brien, Stephen J.] NCI, Lab Genom Divers, NIH, Frederick, MD 21702 USA. [Huang, Shiqiang] Beijing Zoo, Beijing 100044, Peoples R China. [Miller, Philip S.; Traylor-Holzer, Kathy; Seal, Ulysses S.] IUCN World Conservat Unions Species Survival Comm, Conservat Breeding Specialist Grp, Apple Valley, MN 55124 USA. [Wei, Rongping; Zhang, Hemin] China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan Provinc, Peoples R China. [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Xie, Zhong] Chinese Assoc Zool Gardens, Beijing 100037, Peoples R China. [Zhang, Anju] Chengdu Giant Panda Breeding Res Fdn, Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. RP Ballou, JD (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 28 TC 6 Z9 6 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 495 EP 519 DI 10.1017/CBO9780511542244.022 D2 10.2277/ 0521832950 PG 25 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600022 ER PT J AU Wildt, DE Lu, XP Lam, M Zhang, ZH Ellis, S AF Wildt, David E. Lu, Xiaoping Lam, Mabel Zhang, Zhihe Ellis, Susie BE Wildt, DE Zhang, A Zhang, H Janssen, DL Ellis, S TI Partnerships and capacity building for securing giant pandas ex situ and in situ: how zoos are contributing to conservation SO GIANT PANDAS: BIOLOGY, VETERINARY MEDICINE AND MANAGEMENT LA English DT Article; Book Chapter C1 [Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Ellis, Susie] Conservat Int, Washington, DC 20036 USA. [Lam, Mabel] ML Associates LLC, Glastonbury, CT 06033 USA. [Lu, Xiaoping] CITES Management Author China, Beijing 100714, Peoples R China. [Zhang, Zhihe] Chengdu Res Base Giant Panda Breeding, Chengdu 610081, Sichuan Provinc, Peoples R China. RP Wildt, DE (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 8 TC 3 Z9 3 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-83295-3 PY 2006 BP 520 EP 540 DI 10.1017/CBO9780511542244.023 D2 10.2277/ 0521832950 PG 21 WC Biodiversity Conservation; Veterinary Sciences; Zoology SC Biodiversity & Conservation; Veterinary Sciences; Zoology GA BXS85 UT WOS:000296964600023 ER PT S AU Fata, R Kradinov, V Fabricant, D AF Fata, Robert Kradinov, Vladimir Fabricant, Daniel BE Mclean, IS Iye, M TI Flexure mounts for high performance astronomical lenses - art. no. 62695T SO Ground-based and Airborne Instrumentation for Astronomy, Pts 1- 3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Instrumentation for Astronomy CY MAY 25-29, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE lens mounting; large optics; multi-object spectroscopy ID CONVERTED MMT; SPECTROGRAPH; BINOSPEC; OPTICS AB We have developed practical, high performance flexure mounts for large astronomical lenses in the Binospec spectrograph. Flexure mounts are an attractive alternative to the widely used elastomeric tens mounts when high axial stiffness is a priority and coupling fluids are incompatible with elastomers. We describe coupling fluid seals for the flexure mounts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fata, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6334-5 J9 P SOC PHOTO-OPT INS PY 2006 VL 6269 BP T2695 EP T2695 AR 62695T DI 10.1117/12.672634 PN 1-3 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy GA BEZ53 UT WOS:000240348500187 ER PT S AU Fabricant, D Hertz, E Brown, W McLeod, B Angel, R Lloyd-Harth, M AF Fabricant, Daniel Hertz, Edward Brown, Warren McLeod, Brian Angel, Roger Lloyd-Harth, Michael BE Mclean, IS Iye, M TI A wide-field IR spectrograph for the Giant Magellan Telescope - art. no. 62691Z SO Ground-based and Airborne Instrumentation for Astronomy, Pts 1- 3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Instrumentation for Astronomy CY MAY 25-29, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE infrared and multi-object spectroscopy; adaptive optics AB The Giant Magellan Telescope, with seven 8.4 meter primary mirrors, is taking shape as one of the most powerful telescopes of the next generation. We describe a conceptual design for a powerful 0.85 to 2.50 mu m imaging spectrograph that addresses a 7' by 7' field of view for imaging and a 5' by 7' field of view for spectroscopy at the GWT's f/8 Gregorian focus. The all-refractive optical design presses the limits of available lens blank diameters, but delivers excellent images (similar to 0.15" 80% encircled energy) with just four collimator elements and five camera elements. The collimated beam diameter is 300 mm, and the detector is a 6K by 10K array. The spectrograph will use interchangeable slit masks, and an assortment of VPH and conventional surface relief gratings. Each of the entire J, H or K bands can be observed with a resolution of 3000. The scientific potential of ground layer adaptive optics (GLAO) using a constellation of sodium laser guide stars appears to be very high in the near infrared. Simulations suggest that 0.2" FWHM images may be achieved across the entire 7' by 7' field of view of the spectrograph. We describe the design of the GLAO system with a versatile opto-mechanical design that allows rapid changeover between GLAO and seeing-limited observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabricant, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6334-5 J9 P SOC PHOTO-OPT INS PY 2006 VL 6269 BP Z2691 EP Z2691 AR 62691Z DI 10.1117/12.672620 PN 1-3 PG 12 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy GA BEZ53 UT WOS:000240348500066 ER PT S AU Gibbs, K AF Gibbs, Kenneth CA VERITAS Collaboration BE Stepp, LM TI VERITAS: A next generation very high energy gamma-ray telescope - art. no. 62670B SO Ground-based and Airborne Telescopes, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Telescopes CY MAY 24-31, 2006 CL Orlando, FL SP Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE gamma ray; gamma-ray telescope; high-energy astrophysics ID CRAB-NEBULA; TEV; PHOTONS; PROJECT; SYSTEM AB VERITAS (the Very Energetic Radiation Imaging Telescope Array System) is one of a new generation of ground-based gamma-ray observatories. It is being built by a collaboration of ten institutions from Canada, Ireland, the U.K. and the U.S.A.. VERITAS uses the imaging atmospheric Cherenkov technique (IACT) which was developed by the Whipple collaboration using the Whipple 10m telescope. The 10m was the first ground-based gamma-ray telescope to detect both galactic and extragalactic sources of TeV gamma rays. VERITAS is designed to operate in the range from 50 GeV to 50 TeV with optimal sensitivity near 200 GeV; it will effectively overlap with the next generation of space-based gamma-ray telescopes. C1 Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ USA. RP Gibbs, K (reprint author), Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, 6670 Mt Hopkins Rd, Amado, AZ USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6332-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6267 BP B2670 EP B2670 AR 62670B DI 10.1117/12.671514 PN 1&2 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX64 UT WOS:000240018600013 ER PT S AU Hong, J Grindlay, JE Chammas, N Copete, A Baker, RG Barthelmy, SD Gehrels, N Cook, WR Burnham, JA Harrison, FA Collins, J Craig, WW AF Hong, J. Grindlay, J. E. Chammas, N. Copete, A. Baker, R. G. Barthelmy, S. D. Gehrels, N. Cook, W. R. Burnham, J. A. Harrison, F. A. Collins, J. Craig, W. W. BE Franks, LA Burger, A James, RB Barber, HB Doty, FP Roehrig, H TI CZT imaging detectors for ProtoEXIST - art. no. 63190S SO Hard X-Ray and Gamma-Ray Detector Physics and Penetrating Radiation Systems VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Hard X-Ray and Gamma-Ray Detector Physics and Penetrating Radiation Systems VIII CY AUG 14-17, 2006 CL San Diego, CA SP SPIE DE CZT detector; hard X-ray telescope; spectral response AB We describe the detector development for a balloon-borne wide-field hard X-ray (20 - 600 keV) telescope, ProtoEXIST ProtoEXIST is a pathfinder for both technology and science of the proposed implementation of the Black Hole Finder Probe, Energetic X-ray Imaging Survey telescope (EXIST). The principal technology challenge is the development of large area, close-tiled modules of imaging CZT detectors (1000 cm(2) for ProtoEXIST1). We review the updates of the detector design and package concept for ProtoEXIST1 and report the current development status of the CZT detectors, using calibration results of our basic detector unit - 2 x 2 x 0.5 cm CZT crystals with 2.5 mm pixels (8 x 8 array). The current prototype (Rev1) of our detector crystal unit (DCU) shows similar to 4.5 keV electronics noise (FWHM), and the radiation measurements show the energy resolution (FWHM) of the units is 4.7 keV (7.9%) at 59.5 keV, 5.6 keV (4.6%) at 122 keV, and 7.6 keV (2.1%) at 356 keV. The new (Rev2) DCU with revised design is expected to improve the resolution by similar to 30%. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012 NR 9 TC 1 Z9 1 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6398-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6319 BP S3190 EP S3190 AR 63190S DI 10.1117/12.680721 PG 11 WC Instruments & Instrumentation; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Imaging Science & Photographic Technology GA BFI21 UT WOS:000241979600023 ER PT S AU Geary, J Figer, D Gilmore, DK O'Connor, P Oliver, J Radeka, V Stubbs, C Takas, P Tyson, JA AF Geary, J. Figer, D. Gilmore, D. K. O'Connor, P. Oliver, J. Radeka, V. Stubbs, C. Takas, P. Tyson, J. A. BE Dorn, DA Holland, AD TI The LSST sensor technologies studies - art. no. 627601 SO High Energy, Optical, and Infrared Detectors for Astronomy II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on High Energy, Optical, and Infrared Detectors for Astronomy II CY MAY 24-27, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astronomy Inc, Ball Aerosp & Technol Corp, European SE Observat, Opt Infrared Coordinat Network, Particle Phys & Astronomy Res Council, UK Astronomy Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE LSST; sensor; imager; CCD; CMOS AB The LSST project has embarked on an aggressive new program to develop the next generation of silicon imagers for the visible and near-IR spectral regions. In order to better understand and solve some of the technology issues prior to development and mass-production for the huge LSST focal plane, a number of contracts have been written to imager firms to explore specific areas of technology uncertainty. We expect that these study contracts will do much toward reducing risk and uncertainty going into the next phase of development, the prototype production of the final large LSST imager. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Geary, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 NR 1 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6341-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6276 BP 27601 EP 27601 AR 627601 DI 10.1117/12.673291 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BFB08 UT WOS:000240594700003 ER PT S AU Hora, JL Patten, BM Fazio, GG Glaccum, WJ AF Hora, Joseph L. Patten, Brian M. Fazio, Giovanni G. Glaccum, William J. BE Dorn, DA Holland, AD TI The effects of cosmic rays and solar flares on the IRAC detectors: the first two years of in-flight operation - art. no. 62760J SO High Energy, Optical, and Infrared Detectors for Astronomy II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on High Energy, Optical, and Infrared Detectors for Astronomy II CY MAY 24-27, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astronomy Inc, Ball Aerosp & Technol Corp, European SE Observat, Opt Infrared Coordinat Network, Particle Phys & Astronomy Res Council, UK Astronomy Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Spitzer Space Telescope; IRAC; infrared detectors; cosmic rays; image processing and artifacts; space instrumentation ID SPITZER-SPACE-TELESCOPE; INFRARED-ARRAY-CAMERA; PERFORMANCE; ORBIT; CALIBRATION; ASTRONOMY; MISSION; IMAGES; FOCUS AB The Infrared Array Camera (IRAC) is a four-channel camera on the Spitzer Space Telescope, one of three focal plane science instruments. IRAC uses two pairs of 256x256 pixel InSb and Si:As IBC detectors to provide simultaneous imaging at 3.6, 4.5, 5.8, and 8 mu m. IRAC experiences a flux of cosmic rays and solar protons that produce transient effects in science images from each of the arrays, with 4-6 pixels per second being affected during each integration. During extreme solar flares, IRAC experiences a much higher rate of transients which affects the science data quality. We present cosmic ray rates and observed detector characteristics for IRAC during the first two years of science operation, and rates observed in a period of elevated solar proton flux during an intense solar flare in January 2005. We show the changes to the IRAC detectors observed since launch, and assess their impacts to the science data quality. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hora, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-65, Cambridge, MA 02138 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 17 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6341-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6276 BP J2760 EP J2760 AR 62760J DI 10.1117/12.672017 PG 15 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BFB08 UT WOS:000240594700019 ER PT J AU Owsley, DW Ellwood, BB Melton, T AF Owsley, Douglas W. Ellwood, Brooks B. Melton, Terry TI Search for the grave of William Preston Longley, hanged Texas gunfighter SO HISTORICAL ARCHAEOLOGY LA English DT Article AB William Preston Longley was one of the most notorious outlaws in Texas when he was finally tracked down, arrested, and convicted for shooting a boyhood friend. Since he had cheated death before, contemporaries easily believed Longley's hanging in October 1878 was a hoax that allowed him to live and raise a family in Louisiana under an alias. The ultimate test of the hoax hypothesis would be to find Longley's grave and expose either his remains or a weighted coffin. In fall 1992 and spring 1994, a team of scientists used electrical resistivity and magnetometer surveys to locate unmarked burials in areas where historical research indicated Longley's grave may be located. Team members hoped a grainy historic photograph of the marked gravesite could be correlated with a position in the cemetery. The team determined the approximate location of an unmarked grave that could be Longley's. Excavation uncovered the remains of a tall white male, which fit his description, and artifacts recovered from the grave were consistent with those known to have been buried with Longley. Finally, a mitochondrial DNA comparison with his living maternal relative produced a very high probability match. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA. Mitotyping Technol LLC, State Coll, PA 16801 USA. RP Owsley, DW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012,MRC 112, Washington, DC 20013 USA. NR 45 TC 3 Z9 3 U1 2 U2 5 PU SOC HISTORICAL ARCHAEOLOGY PI TUCSON PA PO BOX 30446, TUCSON, AZ 85751-0446 USA SN 0440-9213 J9 HIST ARCHAEOL JI Hist. Archaeol. PY 2006 VL 40 IS 3 BP 50 EP 63 PG 14 WC Archaeology SC Archaeology GA 084UM UT WOS:000240559900005 ER PT J AU Owsley, DW Bruwelheide, KS Cartmell, LW Burgess, LE Foote, SJ Chang, SM Fielder, N AF Owsley, Douglas W. Bruwelheide, Karin S. Cartmell, Larry W., Sr. Burgess, Laurie E. Foote, Shelly J. Chang, Skye M. Fielder, Nick TI The man in the iron coffin: An interdisciplinary effort to name the past SO HISTORICAL ARCHAEOLOGY LA English DT Article ID ISOTOPIC EVIDENCE; DIET; COLLAGEN; DEATH AB The examination of a cast-iron coffin from the Mason family cemetery at Pulaski, Tennessee, offered an exceptional opportunity to study relatively well-preserved human remains, associated artifacts, and the coffin itself. Only a few studies of cast-iron coffins and their contents have incorporated the results of interdisciplinary research in the interpretation of the burial and the remains. The investigation is based on the use of an evolving protocol that promotes the collection of relevant information from several disciplines when evaluating cast-iron coffins and their contents. Multiple lines of evidence identify the remains as those of Isaac Newton Mason, a private in the First Tennessee Confederate Cavalry Regiment, and provide a detailed and intimate glimpse into the past. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, Washington, DC 20013 USA. Valley View Reg Hosp, Dept Pathol, Ada, OK 74820 USA. Natl Museum Amer Hist, Div Social Hist, Washington, DC 20560 USA. Univ Hawaii Manoa, MARC U STAR Program, Honolulu, HI 96822 USA. Tennessee Div Archaeol, Dept Environm & Conservat, Nashville, TN 37211 USA. RP Owsley, DW (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Anthropol, POB 37012,MRC 112, Washington, DC 20013 USA. NR 29 TC 4 Z9 4 U1 0 U2 3 PU SOC HISTORICAL ARCHAEOLOGY PI TUCSON PA PO BOX 30446, TUCSON, AZ 85751-0446 USA SN 0440-9213 J9 HIST ARCHAEOL JI Hist. Archaeol. PY 2006 VL 40 IS 3 BP 89 EP 108 PG 20 WC Archaeology SC Archaeology GA 084UM UT WOS:000240559900008 ER PT S AU Marvin, UB AF Marvin, Ursula B. BE Mccall, GJH Bowden, AJ Howarth, RJ TI Meteorites in history: an overview from the Renaissance to the 20th century SO HISTORY OF METEORITICS AND KEY METEORITE COLLECTIONS: FIREBALLS, FALLS AND FINDS SE Geological Society Special Publication LA English DT Article; Book Chapter ID CAMPO DEL CIELO; CHONDRITE; ARGENTINA; CRATERS AB From ancient times through to the Renaissance reports of stones, fragments of iron and 'six hundred other things' fallen from the sky were written down in books. With few exceptions, these were taken as signals of heaven's wrath. The 18th century Enlightenment brought an entirely new approach in which savants sought rational explanations, based on the laws of physics, for unfamiliar phenomena. They accepted Isaac Newton's dictum of 1718 that outer space must be empty in order to perpetuate the laws of gravitation, and, at the same time, they rejected an old belief that stones can coalesce within the atmosphere. Logically, then, nothing could fall from the skies, except ejecta from volcanoes or objects picked up by hurricanes. They dismissed reports of fallen stones or irons as tales told by superstitious country folk, and ascribed stones with black crusts to bolts of lightning on pyritiferous rocks. The decade between 1794 and 1804 witnessed a dramatic advance from rejection to acceptance of meteorites. The three main contributing factors were E. F. F. Chladni's book of 1794, in which he argued for the actuality of falls and linked them with fireballs; the occurrence of four witnessed and widely publicized falls of stones between 1794 and 1798; and chemical and mineralogical analyses of stones and irons, published in 1802 by Edward C. Howard and Jacques-Louis de Bournon. They showed that stones with identical textures and compositions, very different from those of common rocks, have fallen at different times in widely separated parts of the world. They also showed that erratic masses of metallic iron and small grains of iron in the stones both contain nickel, so they must share a common origin. Meanwhile, in 1789, Anton-Laurent de Lavoisier had revived the idea of the accretion of stones within the atmosphere, which became widely accepted. Its chief rival was a hypothesis that fallen stones were erupted by volcanoes on the Moon. During the first half of the 19th century falls of carbonaceous chondrites and achondrites, and observations on the metallography of irons, provided fresh insights on the range of compositions of meteorite parent bodies. By 1860 both of the two main hypotheses of origins were abandoned, and debates intensified on whether all meteorites were fragments of asteroids or some of them originated in interstellar space. This paper will trace some of the successes and some of the failures that marked the efforts to gain a better understanding of meteorite falls from the end of the 15th century to the early 20th century. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marvin, UB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM umarvin@cfa.harvard.edu NR 209 TC 11 Z9 12 U1 0 U2 0 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-194-9 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2006 VL 256 BP 15 EP 71 DI 10.1144/GSL.SP.2006.256.01.02 PG 57 WC Geology SC Geology GA BKV91 UT WOS:000269439800003 ER PT S AU Clarke, RS Plotkin, H McCoy, TJ AF Clarke, Roy S., Jr. Plotkin, Howard McCoy, Timothy J. BE Mccall, GJH Bowden, AJ Howarth, RJ TI Meteorites and the Smithsonian Institution SO HISTORY OF METEORITICS AND KEY METEORITE COLLECTIONS: FIREBALLS, FALLS AND FINDS SE Geological Society Special Publication LA English DT Article; Book Chapter AB Meteoritics at the Smithsonian Institution is intimately linked to the broader growth of the science, and traces its roots through influential individuals and meteorites from the late 18th century to the dawn of the 21st century. The Institution was founded with an endowment from English mineralogist James Smithson, who collected meteorites. Early work included study of Smithson's meteorites by American mineralogist J. Lawrence Smith and acquisition of the iconic Tucson Ring meteorite. The collection was shaped by geochemist F. W. Clarke and G. P. Merrill, its first meteorite curator, who figured in debate over Meteor Crater and was a US pioneer in meteorite petrology. Upon Merrill's death in 1929, E. P. Henderson would lead the Smithsonian's efforts in meteoritics through a tumultuous period of more than 30 years. Collections growth was spurred by scientific collaborations with S. H. Perry and the Smithsonian Astrophysical Observatory, and a sometimes contentious relationship with H. H. Nininger. Henderson played a key role in increasing meteorite research capabilities after the Second World War, placing the Smithsonian at the forefront of meteoritics. After 1969 involvement in the fall of the Allende and Murchison meteorites, lunar sample analyses, the recovery of the Old Woman meteorite and recovery of thousands of meteorites from Antarctica produced exponential growth of the collection. The collection today serves as the touchstone by which samples returned by spacecraft are interpreted. C1 [Clarke, Roy S., Jr.; McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Plotkin, Howard] Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada. RP Clarke, RS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM rclarke@volcano.si.edu NR 75 TC 4 Z9 4 U1 0 U2 2 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-194-9 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2006 VL 256 BP 237 EP 265 DI 10.1144/GSL.SP.2006.256.01.12 PG 29 WC Geology SC Geology GA BKV91 UT WOS:000269439800013 ER PT S AU McCall, GJH Bowden, AJ Wood, JA Marvin, UB AF McCall, G. J. H. Bowden, A. J. Wood, John A. Marvin, Ursula B. BE Mccall, GJH Bowden, AJ Howarth, RJ TI Epilogue SO HISTORY OF METEORITICS AND KEY METEORITE COLLECTIONS: FIREBALLS, FALLS AND FINDS SE Geological Society Special Publication LA English DT Editorial Material; Book Chapter C1 [Bowden, A. J.] Natl Museums Liverpool, Liverpool L3 8EN, Merseyside, England. [Wood, John A.; Marvin, Ursula B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCall, GJH (reprint author), 44 Robert Franklin Way, Circenester GL7 5UD, Glos, England. EM joemccall@tiscali.co.uk; Alan.Bowden@liverpoolmuseums.org.uk; umarvin@cfa.harvard.edu; Alan.Bowden@liverpoolmuseums.org.uk NR 10 TC 1 Z9 1 U1 0 U2 0 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-194-9 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2006 VL 256 BP 495 EP 504 DI 10.1144/GSL.SP.2006.256.01.24 PG 10 WC Geology SC Geology GA BKV91 UT WOS:000269439800025 ER PT J AU Capper, A Cruz-Rivera, E Paul, V Tibbetts, I AF Capper, A Cruz-Rivera, E Paul, V Tibbetts, I TI Chemical deterrence of a marine cyanobacterium against sympatric and non-sympatric consumers SO HYDROBIOLOGIA LA English DT Article DE Lyngbya majuscula; feeding deterrence; lyngbyatoxin-a; debromoaplysiatoxin; rabbitfish (Siganus fuscescens); sea hare (Stylocheilus striatus) ID HARE STYLOCHEILUS-LONGICAUDA; SECONDARY METABOLITES; LYNGBYA-MAJUSCULA; RABBITFISH SIGANUS; JUVENILE RABBITFISH; NUTRIENT ENRICHMENT; GAIMARD 1824; SEA HARES; TOXINS; PREFERENCES AB This study investigates the influence of mesograzer prior exposure to toxic metabolites on palatability of the marine cyanobacterium, Lyngbya majuscula. We examined the palatability of L. majuscula crude extract obtained from a bloom in Moreton Bay, South East Queensland, Australia, containing lyngbyatoxin-a (LTA) and debromoaplysiatoxin (DAT), to two groups: (1) mesograzers of L. majuscula from Guam where LTA and DAT production is rare; and (2) macro- and mesograzers found feeding on L. majuscula blooms in Moreton Bay where LTA and DAT are often prevalent secondary metabolites. Pair-wise feeding assays using artificial diets consisting of Ulva clathrata suspended in agar (control) or coated with Moreton Bay L. majuscula crude extracts (treatment) were used to determine palatability to a variety of consumers. In Guam, the amphipods, Parhyale hawaiensis and Cymadusa imbroglio; the majid crab Menaethius monoceros; and the urchin Echinometra mathaei were significantly deterred by the Moreton Bay crude extract. The sea hares, Stylocheilus striatus, from Guam were stimulated to feed by treatment food whereas S. striatus collected from Moreton Bay showed no discrimination between food types. In Moreton Bay, the cephalaspidean Diniatys dentifer and wild caught rabbitfish Siganus fuscescens were significantly deterred by the crude extract. However, captive-bred S. fuscescens with no known experience with L. majuscula did not clearly discriminate between food choices. Lyngbya majuscula crude extract deters feeding by most mesograzers regardless of prior contact or association with blooms. C1 Univ Queensland, Sch Life Sci, Ctr Marine Studies, Brisbane, Qld 4072, Australia. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Univ Texas, Inst Marine Sci, Port Aransas, TX 78373 USA. RP Capper, A (reprint author), Univ Queensland, Sch Life Sci, Ctr Marine Studies, Brisbane, Qld 4072, Australia. EM capper@sms.si.edu RI Capper, Angela/B-4403-2012; Tibbetts, Ian/K-6191-2013; OI Tibbetts, Ian/0000-0002-1481-238X; Capper, Angela/0000-0002-4922-0253; Cruz-Rivera, Edwin/0000-0002-5376-9863 NR 35 TC 25 Z9 25 U1 0 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD JAN PY 2006 VL 553 BP 319 EP 326 DI 10.1007/s10750-005-1129-x PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 990GJ UT WOS:000233730900024 ER PT J AU Campbell, BA Campbell, DB AF Campbell, BA Campbell, DB TI Regolith properties in the south polar region of the Moon from 70-cm radar polarimetry SO ICARUS LA English DT Article DE moon; radar; regoliths ID LUNAR POLES; ICE; DEPOSITS; CRATERS AB The south polar region of the Moon contains areas permanently shadowed from solar illumination, which may provide cold traps for volatiles such as water ice. Previous radar studies have emphasized the search for diagnostic polarization signatures of thick ice in areas close to the pole, but near-surface regolith properties and regional geology are also important to upcoming orbital studies of the shadowed terrain. To study regional regolith variations, we collected 70-cm wavelength, 450-m resolution, dual-circular polarization radar data for latitudes 60-90 degrees S using the Arecibo and Greenbank telescopes. The circular polarization ratio, p, is sensitive to differences in rock abundance at the surface and up to tens of m below the surface, depending upon the regolith loss tangent. We observe significant variations in lie, attributed to changes in the surface and subsurface rock population, across the south polar highlands. Concentric haloes of low polarization ratio surrounding Hausen, Morews, and other young craters represent rock-poor ejecta layers. Values of mu(c) up to similar to 1 occur in the floors and near-rim deposits of Eratosthenian and Copernican craters, consistent with abundant rocky ejecta and/or fractured impact melt. Enhanced mu(c) values also correspond to areas mapped as Orientale-derived, plains-forming material [Wilhelms, D.E., Howard, K.A., Wilshire, H.G., 1979. USGS Map I- 1162], and similar polarization properties characterize the permanently shadowed floors of craters Faustini and Shoemaker. Small areas of very high (> 1.5) circular polarization ratio occur on shadowed and seasonally sunlit terrain, and appear to be associated with small craters. We suggest that regolith in low-lying areas near the south pole is characterized by a significant impact melt component from Orientate, which provides a source for excavation of the block-rich ejecta around small craters observed in this and earlier radar studies. The lower portion of the interior wall of Shackleton crater, permanently shadowed from the sun but visible from Earth, is not significantly different in 70-cm scattering properties from diurnally/season ally sunlit areas of craters with similar morphology. (c) 2005 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Cornell Univ, Ithaca, NY 14853 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. EM campbellb@si.edu NR 21 TC 32 Z9 35 U1 0 U2 5 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 JAN PY 2006 VL 180 IS 1 BP 1 EP 7 DI 10.1016/j.icarus.2005.08.018 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400001 ER PT S AU Wellard, S Bingham, G Latvakoski, H Mlynczak, M Johnson, D Jucks, K AF Wellard, S. Bingham, G. Latvakoski, H. Mlynczak, M. Johnson, D. Jucks, K. BE Strojnik, M TI Far-infrared spectroscopy of the troposphere (FIRST): flight performance and data processing - art. no. 62970Q SO Infrared Spaceborne Remote Sensing XIV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Infrared Spaceborne Remote Sensing XIV CY AUG 15-17, 2006 CL San Diego, CA DE interferometer; far-infrared; calibration; water vapor; global energy balance ID LIMB SPECTRAL MEASUREMENTS; CIRRUS CLOUDS; SPECTROMETER AB The radiative balance of the troposphere, and hence global climate, is dominated by the infrared absorption and emission of water vapor, particularly at far-infrared (far-IR) wavelengths from 15-50 mu m. Current and planned satellites observe the infrared region to about 15.4 mu m, ignoring spectral measurement of the far-IR region from 15 to 100 mu m. The far-infrared spectroscopy of the troposphere (FIRST) project, flown in June 2005, provided a balloon-based demonstration of the two key technologies required for a space-based far-IR spectral sensor. We discuss the FIRST Fourier transform spectrometer system (0.6 cm(-1) unapodized resolution), its radiometric calibration in the spectral range from 10 to 100 mu m, and its performance and science data from the flight. Two primary and two secondary goals are given and data presented to show the goals were achieved by the FIRST flight. C1 Utah State Univ, Space Dynam Lab, Logan, UT 84341 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wellard, S (reprint author), Utah State Univ, Space Dynam Lab, Logan, UT 84341 USA. RI Johnson, David/F-2376-2015 OI Johnson, David/0000-0003-4399-5653 NR 20 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6376-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6297 BP Q2970 EP Q2970 AR 62970Q DI 10.1117/12.683976 PG 11 WC Instruments & Instrumentation; Remote Sensing SC Instruments & Instrumentation; Remote Sensing GA BFI35 UT WOS:000241988100021 ER PT J AU Brake, I AF Brake, I TI Diverse Milichiella Giglio-Tos (Diptera : Milichiidae) in Miocene Dominican amber SO INSECT SYSTEMATICS & EVOLUTION LA English DT Article ID KLEPTOPARASITIC FLIES; CHEMICAL ATTRACTION; SPIDERS; CHLOROPIDAE AB Seven new species of Milichiella are described from Dominican amber: M. archaia n. sp., M. dolichosurstyla n. sp., M. dominicana n. sp., M. hennigi n. sp., M. margaretae n. sp., M. guadrisetosa n. sp., and M. theodori n. sp. These species represent the first record of the subfamily Milichiinae in amber and the first descriptions of the family in Dominican amber. The fossil species differ from extant species only in species-level details except M. archaia, which probably belongs to the stemline of Milichiella + Ulia. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Brake, I (reprint author), Smithsonian Inst, Dept Entomol, MRC-0169 NHB,POB 37012, Washington, DC 20013 USA. NR 16 TC 3 Z9 3 U1 1 U2 1 PU APOLLO BOOKS PI STENSTRUP PA KIRKEBY SAND, 19, DK-5771 STENSTRUP, DENMARK SN 1399-560X J9 INSECT SYST EVOL JI Insect Syst. Evol. PY 2006 VL 37 IS 1 BP 17 EP 26 DI 10.1163/187631206788831498 PG 10 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 036OD UT WOS:000237079500002 ER PT J AU Lapolla, JS Schultz, TR Kjer, KM Bischoff, JF AF Lapolla, John S. Schultz, Ted R. Kjer, Karl M. Bischoff, Joseph F. TI Phylogenetic position of the ant genus Acropyga Roger (Hymenoptera : Formicidae) and the evolution of trophophoresy SO INSECT SYSTEMATICS & EVOLUTION LA English DT Article ID HIGHER CLASSIFICATION; DNA-SEQUENCES; TROPHOBIONTS; MUTUALISM; SYMBIOSIS; MEALYBUGS; QUEENS; AMBER AB Trophophoresy is exhibited in two ant genera: Acropyga (Formicinae), in which all 37 species are thought to be trophophoretic, and Tetraponera (Pseudomyrmecinae), in which it has been observed in only one species, T binghami. This study analyses a dataset comprised of both morphological and molecular (D2 region of 28S rRNA and EF1-alpha) data. Evidence is presented in favor of Acropyga being monophyletic, hence trophophoresy has evolved only once within the Formicinae and twice within the ants overall. The data further suggests that Acropyga belongs within a clade containing Anoplolepis, Aphomomyrmex, and Petalomyrmex. Aphomomyrmex and Petalomyrmex were found to be the sister group to Acropyga. The results indicate that the Lasimi and Plagiolepidini are not monophyletic and are in need of reexamination. Given the extant pantropical distribution of Acropyga it is speculated that Acropyga maybe of Gondwanan origin and that trophobiosis was the first form of agriculture to evolve in the ants. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Rutgers State Univ, Dept Ecol & Evolut, New Brunswick, NJ 08901 USA. Natl Ctr Biotechnol Informat, NIH, Bethesda, MD 20892 USA. RP Lapolla, JS (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. EM lapollaj@si.edu; schultz@lab.si.edu; kjer@aesop.rutgers.edu; bischoff@ncbi.nlm.nih.gov FU Intramural NIH HHS [Z01 LM000160-04] NR 38 TC 9 Z9 9 U1 0 U2 12 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1399-560X EI 1876-312X J9 INSECT SYST EVOL JI Insect Syst. Evol. PY 2006 VL 37 IS 2 BP 197 EP 212 DI 10.1163/187631206788831083 PG 16 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 065MT UT WOS:000239164700005 PM 18084637 ER PT J AU Wcislo, WT Gonzalez, VH AF Wcislo, WT Gonzalez, VH TI Social and ecological contexts of trophallaxis in facultatively social sweat bees, Megalopta genalis and M. ecuadoria (Hymenoptera, Halictidae) SO INSECTES SOCIAUX LA English DT Article DE trophallaxis; ritualization; sociality; Megalopta; Halictidae ID EVOLUTION; SOLITARY; ALLOCATION; COLONIES; ANT AB Exchange of liquid food among adults (trophallaxis) is documented for the first time in New World sweat bees (Halictinae). Megalopta genalis and M. ecuadoria are facultatively social, and in social groups foragers regularly give food to the oldest resident female bee, which dominates social interactions. In turn, the oldest resident sometimes re-distributes this food, and shares it with younger foragers. Food is sometimes offered freely, but often the dominant bee exhibits escalating aggressive behavior until she is fed, whereupon she immediately ceases to be aggressive. The occurrence of trophallaxis in a species with mass-provisioned larvae provides an opportunity to examine the ritualization of social behavior. Trophallaxis also increases survivorship of males and females by almost 50 % under experimental conditions, suggesting the behavior is also important in ecological contexts. C1 Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM WcisloW@si.edu; vhgonza@ku.edu RI Gonzalez, Victor/B-4072-2015 NR 42 TC 37 Z9 37 U1 0 U2 9 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 2006 VL 53 IS 2 BP 220 EP 225 DI 10.1007/s00040-005-0861-6 PG 6 WC Entomology SC Entomology GA 058FO UT WOS:000238651100014 ER PT J AU Advani, NK Mueller, UG AF Advani, N. K. Mueller, U. G. TI A preference assay for quantifying symbiont choice in fungus-growing ants (Attini, Formicidae) SO INSECTES SOCIAUX LA English DT Article DE Cyphomyrmex costatus; mutualism; partner choice; symbiont choice; symbiosis ID LEAF-CUTTING ANTS; PARTNER CHOICE; EVOLUTION; COOPERATION; MUTUALISM; SANCTIONS; CONFLICT; RHIZOBIA; AGRICULTURE; MECHANISMS AB We describe a bioassay for the quantification of cultivar preference (symbiont choice) of fungus-growing ants. The bioassay simultaneously presents mycelium of multiple pure cultivar genotypes to worker ants in a cafeteria-style test arena, and preferred versus nonpreferred cultivar genotypes can then be identified based on the ants' quantifiable behavioral tendencies to convert any of the offered mycelium into a fungus garden. Under natural conditions, fungus-growing ants are likely to express such cultivar preferences when mutant cultivars arise in a garden, or when colonies acquire a novel cultivar from a neighboring colony to replace their resident cultivar. We show that workers from different nests of the fungus-growing ant Cyphomyrmex costatus exhibit repeatable preferences vis-a-vis specific cultivar genotypes. The identified preferred and rejected cultivars can then be used in a performance assay to test whether the ants prefer cultivar genotypes that are superior in enhancing colony fitness (measured, for example, as garden productivity or colony growth), as predicted by symbiont-choice theory. C1 Univ Texas, Sect Integrat Biol, Patterson Labs, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Mueller, UG (reprint author), Univ Texas, Sect Integrat Biol, Patterson Labs, 1 Univ Stn C0930, Austin, TX 78712 USA. EM umueller@mail.utexas.edu NR 32 TC 5 Z9 7 U1 2 U2 12 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 2006 VL 53 IS 4 BP 446 EP 455 DI 10.1007/s00040-005-0892-7 PG 10 WC Entomology SC Entomology GA 119FX UT WOS:000242999300010 ER PT J AU Agnarsson, I AF Agnarsson, Ingi TI Phylogenetic placement of Echinotheridion (Araneae : Theridiidae) - do male sexual organ removal, emasculation, and sexual cannibalism in Echinotheridion and Tidarren represent evolutionary replicas? SO INVERTEBRATE SYSTEMATICS LA English DT Article DE cobweb spiders; palpal amputation; theridiid phylogeny ID SPIDERS ARANEAE; MAXIMUM-LIKELIHOOD; ANELOSIMUS ARANEAE; MITOCHONDRIAL-DNA; COBWEB SPIDERS; REVISION; SUBSTITUTION; ORBICULARIAE; MADAGASCAR; ARANEOIDEA AB Uniquely among spiders, males of two cobweb spider (Theridiidae) genera, Tidarren Chamberlin & Ivie, 1934 and Echinotheridion Levi, 1963, voluntarily amputate one of their secondary sexual organs ( the pedipalpi, modified as sperm transfer organs) before their last molt and thus have only one palp as adults. This is the first step in a fascinating sexual biology observed in both genera, which is marked by sexual dimorphism males are tiny compared with females - and usually involves both emasculation and sexual cannibalism. To study the evolution of these striking traits it is essential to understand the phylogenetic relationship of these genera. Both morphological and molecular data place Tidarren in the subfamily Theridiinae. However, Echinotheridion has not been placed phylogenetically to date owing to rarity of specimens, and difficulty of interpreting the highly autapomorphic palpal organ, the main source of morphological characters. Here, the phylogenetic position of Echinotheridion is inferred using fragments of three nuclear (Histone 3, 18S rDNA, and 28S rDNA) and two mitochondrial (16S rDNA and COI) loci. Each matrix separately, and a combined matrix, were analysed using parsimony with gaps either treated as missing data, or as 5th state, and with Bayesian methods. Although all genes agree that Tidarren and Echinotheridion are closely related, perhaps surprisingly, none of the analyses supported their sister relationship. The sister relationship was ambiguously supported in a preliminary morphological analysis, whereas combined molecular and morphological data refuted it. This implies a more complex evolutionary history of male sexual organ removal and other bizarre sexual biology of Tidarren and Echinotheridion than previously envisioned. Many of the analyses are equally consistent with two hypotheses: a single origin, followed by a secondary loss; or independent evolution of this behaviour in the two genera. However, based on the combined molecular Bayesian phylogeny, and some of the preliminary 'total evidence' analyses, the latter hypothesis is better supported. C1 Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Dept Entomol, 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 NR 37 TC 13 Z9 13 U1 2 U2 8 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-5226 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2006 VL 20 IS 4 BP 415 EP 429 DI 10.1071/IS05043 PG 15 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 078EP UT WOS:000240085000001 ER PT J AU Kuntner, M Alvarez-Padilla, F AF Kuntner, Matjaz Alvarez-Padilla, Fernando TI Systematics of the Afro-macaronesian spider genus Sancus (Araneae, Tetragnathidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Tetragnathidae; Sancus; Leucognatha; taxonomy; phylogenetics; biogeography ID PHYLOGENY; NEPHILIDAE; ARANEIDAE AB We review the systematics of the tetragnathid spider genus Sancus Tullgren, hitherto known from a single species from Kilimanjaro. The type species Sancus bilineatus Tullgren is redescribed and diagnosed from the only other known species, S. acoreensis (Wunderlich) new combination. Leucognatha Wunderlich is a junior synonym of Sancus, which thus eliminates two monotypic tetragnathid genera. A phylogenetic analysis of 15 tetragnathid and eight outgroup genera confirms the monophyly of Sancus and places it precisely in Tetragnathidae. We discuss the phylogenetic relationships among tetragnathid genera and the peculiar biogeography of Sancus, now known from east African mountains (Kilimanjaro and Mt. Kenya) and from the Azores in the northeastern Atlantic. C1 George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Sci Res Ctr, Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. NR 32 TC 7 Z9 8 U1 1 U2 4 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLADG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 1 BP 113 EP 125 DI 10.1636/H04-27.1 PG 13 WC Entomology SC Entomology GA 081GA UT WOS:000240304000010 ER PT J AU Eberhard, WG AF Eberhard, William G. TI Dispersal by Ummidia spiderlings (Araneae, Ctenizidae): Ancient roots of aerial webs and orientation? SO JOURNAL OF ARACHNOLOGY LA English DT Article DE mygalomorph ballooning behavior; orientation ID NATURAL-HISTORY; ATYPIDAE C1 Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Costa Rica. Univ Costa Rica, Escuela Biol, Ciudad Univ, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, Costa Rica. NR 23 TC 2 Z9 3 U1 1 U2 7 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLADG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 1 BP 254 EP 257 DI 10.1636/S03-54.1 PG 4 WC Entomology SC Entomology GA 081GA UT WOS:000240304000030 ER PT J AU Kuntner, M Levi, HW AF Kuntner, Matjaz Levi, Herbert W. TI Nephila hirta, a new synonym of Eustala fuscovittata (Araneae, Araneidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Nephila; Nephilengys; Nephilinae; Tetragnathidae; Araneidae; taxonomy; French Guiana AB Nephila ?hil-to Taczanowski 1873 was described from French Guiana, but is currently listed under Nephilengys L. Koch. It is here redescribed and transferred from Nephilinae (Tetragnathidae)* to the araneid,enus Eusiala Simon, and proposed as a junior synonym of E. fuscovittota (Keyserling 1864). Eustala appears to be the most speciose American araneid genus and is in need of revision. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Kuntner, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC USA. EM kuntner@gmail.com NR 20 TC 1 Z9 2 U1 0 U2 0 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 2 BP 444 EP 447 DI 10.1636/H05-14 SC.1 PG 4 WC Entomology SC Entomology GA 140KT UT WOS:000244504600015 ER PT J AU Jaffe, R Eberhard, W De Angelo, C Eusse, D Gutierrez, A Quijas, S Rodriguez, A Rodriguez, M AF Jaffe, Rodolfo Eberhard, William De Angelo, Carlos Eusse, Diana Gutierrez, Adrian Quijas, Sandra Rodriguez, Antonio Rodriguez, Mayanin TI Caution, webs in the way! Possible functions of silk stabilimenta in Gasteracantha cancriformis (Araneae, Araneidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE orb webs; silk stabilimenta; spiders; warning; prey attraction; camouflage ID SPIDERS; PREY AB We tested three hypotheses concerning the function of stabilimenta in the orb weaver Gasteracantha cancritformis: 1) warning to large animals that might accidentally destroy the web; 2) prey attraction; and 3) camouflage. One prediction of the warning hypothesis (but not of the others), that less exposed webs should have fewer stabilimentum tufts, was verified: very few tufts occurred on the peripheral lines of small webs. On the other hand, a prediction of the prey attraction hypothesis, that webs with more stabilimentum tufts should also have more captured prey, was only confirmed in one sub sample, and further analysis indicated that spider size rather than number of stabilimentum tufts best explained the presence of prey. An additional observation not in accord with prey attraction was that resting webs, which lacked sticky silk for prey capture, nevertheless had abundant stabilimentum tufts. Finally, the number of stabilimentum tufts was lower in the webs of white (as opposed to yellow or orange) spiders, contradicting a prediction of the camouflage hypothesis. The strongest conclusions from our results are support for the warning function, and lack of support for the prey attraction function. C1 Univ Halle Wittenberg, Inst Biol, D-06099 Halle, Germany. Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Fundac Vida Silvestre Argent, Iguazu, Argentina. Univ Valle, Cali, Colombia. Natl Autonomous Univ Mexico, Mexico City, DF, Mexico. Natl Autonomous Univ Mexico, Ctr Invest & Ecosistemas, Yucatan, Mexico. Univ La Habana, Fac Biol, Grp Ecol Vertebrados, Havana, Cuba. Univ Los Andes, Merida, Venezuela. RP Jaffe, R (reprint author), Univ Halle Wittenberg, Inst Biol, Hoher Weg 4 125, D-06099 Halle, Germany. EM rodolfojaffe@zoologie.uni-halle.de RI Jaffe, Rodolfo/K-3230-2013; OI Jaffe, Rodolfo/0000-0002-2101-5282 NR 17 TC 12 Z9 13 U1 1 U2 4 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 2 BP 448 EP 455 DI 10.1636/S04-28.1 PG 8 WC Entomology SC Entomology GA 140KT UT WOS:000244504600016 ER PT J AU Jorger, KM Eberhard, WG AF Jorger, Katharina M. Eberhard, William G. TI Web construction and modification by Achaearanea tesselata (Araneae, Theridiidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE web construction behavior; web design; aerial sheet web; cobweb spider ID PHYLOGENETIC IMPLICATIONS; SYNOTAXUS ARANEAE; BUILDING BEHAVIOR; SPIDERS ARANEAE; TETRAGNATHIDAE; ARANEOIDEA; COMB AB The web construction behavior of Achaearanea tesselata (Keyserling 1884) was observed in the field and in captivity using Suspended wire frames that allowed detailed observations. Construction included three stages: preliminary exploration during which lines were broken, reeled up, and replaced; construction of anchor lines and the upper tangled and construction and then filling in of the sheet below the bangle. Repeated visits to the Mouth of the retreat during tangle construction resulted in the apparent reinforcement of the few lines radiating from this area, a possible adaptation to sense the location of prey in the web, and to facilitate orientation of the spider to prey in the web. Filling in the sheet, which alternated with additions to the tangle, included two previously undescribed behavioral patterns: irregular wandering on the sheet and apparent attachments of the dragline using only the two legs IV to hold previous lines against the spinnerets. The spider needed 1-2 nights, working several hours each night, to make a complete tangle and sheet and added lines and extended both the tangle and the sheet on subsequent nights. Spiders adapted the shapes of their webs to their surroundings. C1 Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Jorger, KM (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM k_joerger@hotmail.com NR 30 TC 7 Z9 7 U1 1 U2 3 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 3 BP 511 EP 523 DI 10.1636/S05-30.1 PG 13 WC Entomology SC Entomology GA 158EA UT WOS:000245772800003 ER PT J AU Agnarsson, I Coddington, JA AF Agnarsson, Ingi Coddington, Jonathan A. TI Notes on web and web plasticity and description of the male of Achaearanea hieroglyphica (Mello-Leitao) (Araneae, Theridiidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE orbicularia; spider webs; taxonomy; web evolution ID SPIDERS AB Cobweb spiders (Theridiidae) exhibit a rich variety of web designs. Current knowledge of theridiid web architecture and evolution indicates that theridiid web design shows high within-taxon diversity and frequent convergence. Here we redescribe Achaearanea hieroglyphica (Mello-Leitao 1940), including the first description of the male, and document in this species (1) an unusual web design and (2) two dramatically different type of webs. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. RP Agnarsson, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, NHB-105,POB 37012, Washington, DC 20013 USA. EM iagnarsson@gmail.com NR 12 TC 5 Z9 5 U1 0 U2 2 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 3 BP 638 EP 641 DI 10.1636/06-26.1 PG 4 WC Entomology SC Entomology GA 158EA UT WOS:000245772800018 ER PT J AU Coddington, JA Agnarsson, I AF Coddington, Jonathan A. Agnarsson, Ingi TI Subsociality in Helvibis thorelli keyserling 1884 (Araneae, Theridiidae, Theridiinae) from French Guiana SO JOURNAL OF ARACHNOLOGY LA English DT Article DE evolution of sociality; maternal care; communal feeding ID ANELOSIMUS ARANEAE; PHYLOGENETIC ANALYSIS; STEGODYPHUS-LINEATUS; SPIDERS ARANEAE; MATERNAL-CARE; SOCIALITY; WEB; ARANEOIDEA; REVISION; ERESIDAE AB Preliminary observations on Helvibis thorelli (Theridiidae) in French Guiana suggest a typical subsocial behavior in this species, with nests consisting of a mother and her offspring who collaborate in prey capture. Communal feeding occurs over several juvenile instars. Subsociality has previously been described in three theridiid genera (Achaearanea, Anelosimus, Theridion) and predicted to occur in further genera of the subfamily Theridiinae. Our findings support this prediction and have important implications for comparative Studies as they add another independent observation of social behavior: current phylogenetic knowledge implies subsociality evolved independently in each of these genera. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. RP Agnarsson, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, NHB-105,POB 37012, Washington, DC 20013 USA. EM iagnarsson@gmail.com NR 20 TC 5 Z9 5 U1 0 U2 4 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2006 VL 34 IS 3 BP 642 EP 645 DI 10.1636/05-84.1 PG 4 WC Entomology SC Entomology GA 158EA UT WOS:000245772800019 ER PT J AU Linton, ET Atkins, RW Badran, HM Blaylock, G Boyle, PJ Buckley, JH Byrum, KL Carter-Lewis, DA Celik, O Chow, YCK Cogan, P Daniel, MK Dowdall, C Falcone, AD Fegan, DJ Fegan, SJ Finley, JP Fortin, P Guiterrez, KJ Hall, J Hanna, D Holder, J Horan, D Hughes, SB Humensky, TB Jung, I Kenny, GE Kertzman, M Kieda, DB Kildea, J Knapp, J Krawczynski, H Lang, MJ LeBohec, S Maier, G Moriarty, P Ong, RA Perkins, JS Pizlo, F Pohl, M Quinn, J Ragan, K Rebillot, PF Reynolds, PT Sembroski, GH Steele, D Swordy, SP Valcarcel, L Wakely, SP Weekes, TC White, RJ AF Linton, ET Atkins, RW Badran, HM Blaylock, G Boyle, PJ Buckley, JH Byrum, KL Carter-Lewis, DA Celik, O Chow, YCK Cogan, P Daniel, MK Dowdall, C Falcone, AD Fegan, DJ Fegan, SJ Finley, JP Fortin, P Guiterrez, KJ Hall, J Hanna, D Holder, J Horan, D Hughes, SB Humensky, TB Jung, I Kenny, GE Kertzman, M Kieda, DB Kildea, J Knapp, J Krawczynski, H Lang, MJ LeBohec, S Maier, G Moriarty, P Ong, RA Perkins, JS Pizlo, F Pohl, M Quinn, J Ragan, K Rebillot, PF Reynolds, PT Sembroski, GH Steele, D Swordy, SP Valcarcel, L Wakely, SP Weekes, TC White, RJ TI A new search for primordial black hole evaporations using the Whipple gamma-ray telescope SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE gamma ray bursts; black holes ID COSMIC-RAYS; BURSTS; MATTER; SCALE AB Stephen Hawking's prediction that black holes should radiate like black bodies has several important consequences, including the possibility of the detection of small (similar to 10(15) g) black holes created in the very early universe. The detection of such primordial black holes ( PBHs) would be an important discovery, not only confirming Hawking's theory, but also providing valuable insights into the history of the early universe. A search through 5.5 years of archival data from the Whipple Atmospheric Cerenkov Telescope is made for TeV gamma-ray bursts on 1, 3, and 5 s timescales. On the basis of a null result from this direct search for PBH evaporations, an upper limit of 1.08 x 10(6) pc(-3) yr(-1) (99% CL) is set on the PBH evaporation rate in the local region of the galaxy, assuming the Standard Model of particle physics. This is more than a factor of two better than the previous limit at this energy range and includes longer timescales than have previously been explored. Comparison of this result with previous limits on the fraction of the critical density comprised by PBHs, Omega(pbh), depends strongly on assumptions made about PBH clustering; in models predicting strong PBH clustering, the limit in this work could be as many as ten orders of magnitude more stringently than those set by diffuse MeV gamma-ray observations. C1 Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Argonne Natl Lab, Argonne, IL 60439 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. RP Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. EM etl@uchicago.edu OI Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 22 TC 12 Z9 12 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD JAN PY 2006 IS 1 AR 013 DI 10.1088/1475-7516/2006/01/013 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 008MR UT WOS:000235045400014 ER PT J AU El-Reefy, HI Sharshar, T Zaghloul, R Badran, HM AF El-Reefy, HI Sharshar, T Zaghloul, R Badran, HM TI Distribution of gamma-ray emitting radionuclides in the environment of Burullus Lake: I. Soils and vegetations SO JOURNAL OF ENVIRONMENTAL RADIOACTIVITY LA English DT Article DE soil; vegetation; Burullus Lake; Egypt; caesium-137; radium-226; thorium-232; potassium-40 ID NATURAL RADIOACTIVITY; NILE DELTA; ANTHROPOGENIC RADIONUCLIDES; CHERNOBYL ACCIDENT; SHORELINE EROSION; VOLCANIC ISLAND; FALLOUT CS-137; CACERES SPAIN; SAND SAMPLES; SOUTH-INDIA AB The concentrations and distribution of gamma-ray emitting isotopes in Burullus Lake were investigated with the aim of evaluating the environmental radioactivity. Particularly in wetlands, natural properties of the environment can cause the actual inventory to be different from the activity originally deposited. The mean concentrations of Ra-226, Th-232 and K-40 were 14.3, 15.5 and 224 Bq/kg, respectively, in the coastal soils. On the other hand, soil samples from the islands had mean concentrations of 13.5, 17.4 and 341 Bq/ka for Ra-226, Th-232 and K-40, respectively. Samples from coast and islands show evidence of possible transfer and accumulation of the Cs-137 radionuclide. The mean Cs-137 activity concentrations in the soil samples were 1.2 and 15.1 Bq/kg in the coast and islands, respectively. The vertical migration Of Cs-137 was studied based on its content in the consequently located three soil layers down to 30 cm depth. The radium equivalent, dose rate in air and annual dose equivalent from the terrestrial natural gamma-radiation were evaluated. The mean activity concentrations of the gamma-ray emitting radionuclides in vegetation were relatively low. (C) 2005 Elsevier Ltd. All rights reserved. C1 Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Atom Energy Author, Hot Labs Ctr, Cairo, Egypt. Tanta Univ, Fac Educ, Dept Chem & Phys, Kafr El Shaikh, Egypt. Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Badran, HM (reprint author), Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. EM hussein_badran@hotmail.com NR 71 TC 29 Z9 30 U1 1 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-931X J9 J ENVIRON RADIOACTIV JI J. Environ. Radioact. PY 2006 VL 87 IS 2 BP 148 EP 169 DI 10.1016/j.jenvrad.2005.11.006 PG 22 WC Environmental Sciences SC Environmental Sciences & Ecology GA 026MP UT WOS:000236343300002 PM 16427723 ER PT J AU Vance, DJ Culver, SJ Corbett, DR Buzas, MA AF Vance, DJ Culver, SJ Corbett, DR Buzas, MA TI Foraminifera in the Albemarle Estuarine System, North Carolina: Distribution and recent environmental change SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID SALT-MARSH FORAMINIFERA; BENTHIC FORAMINIFERA; ASSEMBLAGES; POPULATIONS; GEORGIA; ISLAND; USA AB This study investigated the surface and subsurface distributions of foraminifera (both live populations and dead assemblages) throughout the Albemarle Estuarine System (AES) to determine the utility of the modern foraminiferal assemblages as models for paleoenvironmental interpretations in this estuarine and barrier island system. Thirty-seven species were recognized in the dead assemblages from 49 stations; 19 species comprised the living populations. Cluster analysis of the dead assemblages defined five biofacies: the calcareous foraminiferal nearshore marine and inlet biofacies, and the dominantly agglutinated foraminiferal estuarine shoal, estuary, inner estuary, and marsh biofacies. Paleoenvironmental reconstruction of three cores from the central Albemarle basin, based on the distribution of dead surface foraminiferal assemblages, recognized the inner estuarine and estuarine biofacies. Radionuclide tracers (Ph-210 and Cs-137) provided the geochronologic framework for each core. The westernmost core was capped by the inner estuarine biofacies overlying the estuarine biofacies, indicating either accumulation of a seasonal ephemeral layer of sediment from a lower brackish, upstream environment or increased freshwater discharge since the 1990's as a result of increased tropical storm and hurricane activity. The two easternmost cores indicated that, in the early 19(th) century, Albemarle Sound populations included calcareous foraminiferal species. These taxa were adapted to the higher salinities that resulted from several inlets that were open adjacent to the AES prior to 1828. Taphonomic processes (test transport, test dissolution, mechanical test breakage) are active but, with the exception of test dissolution in a relatively restricted geographic area, they do not significantly alter surficial foraminiferal assemblages in the transition into subfossil assemblages. Thus, foraminiferal distributions are useful for characterizing modern estuarine environments and for interpreting paleoenvironmental changes in sediments deposited over the past few hundred years in coastal North Carolina. C1 E Carolina Univ, Dept Geol, Greenville, NC 27858 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Vance, DJ (reprint author), E Carolina Univ, Dept Geol, Greenville, NC 27858 USA. EM culvers@mail.ecu.edu NR 74 TC 35 Z9 36 U1 0 U2 7 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 JAN PY 2006 VL 36 IS 1 BP 15 EP 33 DI 10.2113/36.1.15 PG 19 WC Paleontology SC Paleontology GA 016CP UT WOS:000235598600003 ER PT J AU Santos, C Norenburg, JL Bueno, SLS AF Santos, Cynthia Norenburg, Jon L. Bueno, Sergio L. S. TI Three new species of Carcinonemertes (Nemertea, Carcinonemertidae) from the southeastern coast of Brazil SO JOURNAL OF NATURAL HISTORY LA English DT Article; Proceedings Paper CT 6th International Conference on Nemertean Biology CY JUN 21, 2004 CL Weber State Univ, Ogden, UT HO Weber State Univ DE Carcinonemertidae; decapod crustacean; symbiosis; predation; Carcinonemertes divae; Carcinonemertes caissarum; Carcinonemertes sebastianensis; Brazil ID SYMBIOTIC EGG PREDATOR; N-SP NEMERTEA; HOST; CRUSTACEA; AUSTRALIA; DECAPODA; CRAB; INFESTATION; ADAPTATIONS; PARASITES AB Three new species of Carcinonemertes from the southeastern coast of Brazil are described: Carcinonemertes divae new species, Carcinonemertes caissarum new species and Carcinonemertes sebastianensis new species. They were found, respectively, associated with the crabs Libinia spinosa, Hepatus pudibundus and Menippe nodifrons, each a newly recorded host for Carcinonemertes. Characters not previously used to describe members of the family Carcinonemertidae, such as distance from ovaries to tip of head, distance from brain to tip of head and distance from stylet to tip of head are included in the descriptions of the new species and are discussed. The locations of these new carcinonemertid worms in their respective hosts are presented in detail and a novelty regarding the infestation site is registered. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05508900 Sao Paulo, Brazil. RP Santos, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, POB 37012,W-216,MRC 163, Washington, DC 20013 USA. EM sancynthia@gmail.com RI Bueno, Sergio/D-7391-2012; Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 18 TC 4 Z9 5 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2006 VL 40 IS 15-16 BP 915 EP 930 DI 10.1080/00222930600833842 PG 16 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 083CY UT WOS:000240434700003 ER PT J AU Ritger, RK Norenburg, JL AF Ritger, Rebecca Kirk Norenburg, Jon L. TI Tubulanus riceae new species (Nemertea : Anopla : Palaeonemertea : Tubulanidae), from south Florida, Belize and Panama SO JOURNAL OF NATURAL HISTORY LA English DT Article; Proceedings Paper CT 6th International Conference on Nemertean Biology CY JUN 21, 2004 CL Weber State Univ, Ogden, UT HO Weber State Univ DE Nemertea; Tubulanidae; taxonomy; littoral; worms; anatomy AB Specimens of Tubulanus riceae new species (Nemertea: Palaeonemertea) were collected from a Phragmatopoma worm reef in the surf zone at Fort Pierce ( Florida, USA) and from sublittoral rubble at Carrie Bow Cay ( Belize) and Bocas del Toro ( Panama). They have well-developed lateral sensory organs, form a cellophane-like tube and appear to have ocelli-like structures. The latter, if confirmed as ocelli, would be the first reported for a tubulanid. The new species is characterized by a unique color pattern, resembling that of Tubulanus rhabdotus, but it is distinctive in its milky-tan ground color with annular bands of brown pigment bounded by white margins and in having up to six to eight dorsal, longitudinal, but broken, reflective white stripes. C1 American Univ, Washington, DC 20016 USA. Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Norenburg, JL (reprint author), Smithsonian Inst, NMNH, POB 37012,W-216,MRC163, Washington, DC 20013 USA. EM norenburgj@si.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 20 TC 6 Z9 8 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2006 VL 40 IS 15-16 BP 931 EP 942 DI 10.1080/00222930600833867 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 083CY UT WOS:000240434700004 ER PT J AU Santos, C Bueno, SLS Norenburg, JL AF Santos, Cynthia Bueno, Sergio L. S. Norenburg, Jon L. TI Infestation by Carcinonemertes divae (Nemertea : Carcinonemertidae) in Libinia spinosa (Decapoda : Pisidae) from Sao Sebastiao Island, SP, Brazil SO JOURNAL OF NATURAL HISTORY LA English DT Article; Proceedings Paper CT 6th International Conference on Nemertean Biology CY JUN 21, 2004 CL Weber State Univ, Ogden, UT HO Weber State Univ DE infestation; symbionts; Carcinonemertes divae; Libinia spinosa; Brazil ID EGG PREDATOR; SPIDER CRAB; HEMIGRAPSUS-OREGONENSIS; METHYL FARNESOATE; SHORE CRAB; HOST; EMARGINATA; EPIALTI; PARASITOLOGY; ADAPTATIONS AB Nemerteans of the genus Carcinonemertes are obligate symbiotic egg predators of many decapod crustaceans. This study presents the prevalence and intensity of infestation by Carcinonemertes divae in the crab, Libinia spinosa, from Sao Sebastiao Island, Sao Paulo State, Brazil. Overall prevalence of infestation was 69.2% and mean intensity of infestation was 20.8 +/- 3.4 ( range: 1-148). Significant differences in prevalence and mean intensity of infestation were observed between males and females and between ovigerous and non-ovigerous adult females of Libinia spinosa. Prevalence and mean intensity of infestation did not differ significantly between juvenile and adult crabs or among ovigerous crabs with eggs in different stages of embryogenesis. Carapace width of male crabs was negatively correlated with prevalence of infestation by Carcinonemertes divae. Sexual contact appeared to be a source of transmission of worms between males and females of Libinia spinosa. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. Univ Sao Paulo, Dept Zool, Inst Biociencias, BR-05508900 Sao Paulo, Brazil. RP Santos, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, W-216,MRC 163,POB 37012, Washington, DC 20013 USA. EM sancynthia@gmail.com RI Bueno, Sergio/D-7391-2012; Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 21 TC 5 Z9 6 U1 0 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2006 VL 40 IS 15-16 BP 999 EP 1005 DI 10.1080/00222930600834105 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 083CY UT WOS:000240434700008 ER PT J AU Anker, A Poddoubtchenko, D Marin, IN AF Anker, Arthur Poddoubtchenko, Denis Marin, Ivan N. TI On the presence of the alpheid shrimp genus Bermudacavis Anker and Iliffe, 2000 (Crustacea : Decapoda : Caridea) in the Pacific Ocean, with description of a new species from Vietnam SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Alpheidae; Bermudacaris; commensalism; inverted chelipeds; new genus diagnosis; new species AB Bermudacaris britayevi n. sp. is described on the basis of a single specimen collected from a burrow, presumably of a callianassid ghost-shrimp, on an intertidal sand-mud flat of Dam Bay of Tre Island, Nha Trang Bay, Vietnam, and is the first record of Bermudacaris in the Pacific Ocean. The new species differs ecologically from the two previously described species, B. harti Anker and Iliffe, 2000 from the anchialine caves of Bermuda in the western Atlantic Ocean, and B. australiensis Anker and Komai, 2004 collected in the western Indian Ocean off northwestern Australia. The original diagnosis of Bermudacaris Anker and Iliffe, 2000 is emended. A key to the three species of Bermudacaris is provided. C1 Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. Russian Acad Sci, AN Severtsov Inst Ecol & Evolut, Lab Ecol & Morphol Marine Invertebrates, Moscow, Russia. RP Anker, A (reprint author), Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. EM ankera@edu.si NR 6 TC 2 Z9 6 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PY 2006 VL 40 IS 27-28 BP 1675 EP 1686 DI 10.1080/00222930600937734 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 109AW UT WOS:000242281300003 ER PT J AU Agnarsson, I Barrantes, G May-Collado, LJ AF Agnarsson, I. Barrantes, G. May-Collado, L. J. TI Notes on the biology of Anelosimus pacificus Levi, 1963 (Theridiidae, Araneae) - evidence for an evolutionary reversal to a less social state SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Anelosimus pacificus; Araneae; behaviour; evolution of sociality; Theridiidae ID PHYLOGENETIC ANALYSIS; SPIDER; REVISION; ERESIDAE AB All hitherto studied Anelosimus species are social, either temporarily (subsocial) or permanently (quasisocial); the genus represents the largest known clade of social spiders. We provide behavioural data on Anelosimus pacificus Levi, 1956 (Theridiidae, Araneae) a species that hitherto was known from only a few specimens collected half a century ago. Anelosimus pacificus, unlike its better known congeners, is solitary for the majority of its lifespan with the juveniles passively receiving maternal care before dispersal at an early instar. Given the phylogenetic position of A. pacificus, this is an example of a behavioural reversal to a less social (solitary) state, and the first such reversal documented in spiders. Interestingly, linked with this is a reversal in other traits. Anelosimus pacificus web architecture, use of sticky silk, the ability of juveniles to emerge from the egg sac, and build and maintain webs without help from the mother, all more resemble traits in typical solitary theridiids than those in its social congeners. These observations may help elucidate what factors contribute to the evolution of sociality in spiders. C1 Univ British Columbia, Dept Zool, Vancouver, BC, Canada. Univ British Columbia, Dept Bot, Vancouver, BC, Canada. Smithsonian Inst, Washington, DC USA. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. Florida Int Univ, Dept Sci Biol, Miami, FL USA. RP Agnarsson, I (reprint author), Univ British Columbia, Dept Zool, 3529-6270 Univ Blvd, Vancouver, BC, Canada. EM iagnarsson@gmail.com NR 18 TC 8 Z9 8 U1 0 U2 11 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0022-2933 EI 1464-5262 J9 J NAT HIST JI J. Nat. Hist. PY 2006 VL 40 IS 47-48 BP 2681 EP 2687 DI 10.1080/00222930601110752 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 135JC UT WOS:000244148900005 ER PT J AU Cheetham, AH Sanner, J Taylor, PD Ostrovsky, AN AF Cheetham, AH Sanner, J Taylor, PD Ostrovsky, AN TI Morphological differentiation of avicularia and the proliferation of species in mid-cretaceous Wilbertopora Cheetham, 1954 (Bryozoa : Cheilostomata) SO JOURNAL OF PALEONTOLOGY LA English DT Article ID EVOLUTIONARY SIGNIFICANCE; TEMPO AB Discovery of avicularium-like polymorphs in Wilbertopora mutabilis Cheetham, 1954 has provided not only a new opportunity for revising the genus Wilbertopora Cheetham, 1954, but also a more detailed basis for documenting the series of morphological changes by which avicularia differentiated from ordinary feeding zooids in what appears to be the first occurrence of these characteristic cheilostome bryozoan structures in the fossil record. Eighteen of a total 60 quantitative characters measured on avicularia and ordinary and ovicell-bearing autozooids were sufficient to distinguish eight species of Wilbertopora by discriminant function analysis of zooid data from 93 colonies from the mid-Cretaceous (Albian-Cenomanian) Washita Group in northeastern Texas and southeastern Oklahoma. Eighteen of a total of 20 of the quantitative characters that could be statistically coded for cladistic analysis proved to be informative with respect to parsimony, providing two maximally parsimonious trees for the eight species. Two-thirds of the diagnostic characters involve avicularia. An additional 55 colonies too poorly preserved for morphometric analysis could then be assigned to species qualitatively, with 170 more colonies lacking species-diagnostic characters. The cladistic trees strongly suggest that most or all of the species diverged before the end of the Albian, but stratigraphic resolution is insufficient to test this hypothesis. Nevertheless, the series of morphological changes differentiating avicularia from ordinary autozooids in these species, based on the cladistic relationships, is highly significant statistically, and may be a pattern later repeated in other cheilostomes. Wilbertopora and W. mutabilis are emended, and seven new species are described: W. listokinae, W tappanae, W. spatulifera, W attenuata, W improcera, W. acuminata, and W. hoadleyae. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC USA. Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. St Petersburg State Univ, Fac Biol & Soil Sci, Dept Invertebrate Zool, St Petersburg 199034, Russia. RP Cheetham, AH (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC USA. EM cheetham@si.edu; sannerj@si.edu; pdt@nhm.ac.uk; oan_univer@yahoo.com RI Ostrovsky, Andrew/D-6439-2012 OI Ostrovsky, Andrew/0000-0002-3646-9439 NR 43 TC 28 Z9 29 U1 1 U2 5 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 JAN PY 2006 VL 80 IS 1 BP 49 EP 71 DI 10.1666/0022-3360(2006)080[0049:MDOAAT]2.0.CO;2 PG 23 WC Paleontology SC Paleontology GA 997FV UT WOS:000234231500004 ER PT J AU Kiel, S AF Kiel, S TI New records and species of molluscs from tertiary cold-seep carbonates in Washington State, USA SO JOURNAL OF PALEONTOLOGY LA English DT Review ID HYDROTHERMAL VENTS; WESTERN WASHINGTON; DEEP-SEA; SOUTHWESTERN WASHINGTON; OLIGOCENE ROCKS; CHEMOSYNTHETIC-COMMUNITY; COCCULINIFORM LIMPETS; HUMPTULIPS FORMATION; METHANE SEEPS; NEW-ZEALAND AB Eighteen gastropod and seven bivalve species are reported from Eocene to Oligocene cold-seep carbonates in Washington State, USA. Four species are new (Niso littlei, Turrinosyrinx hickmanae, Xanthodaphne? campbellae, and Lurifax goederti), and 16 described in open nomenclature. Previously unknown features of protoconch or prodissoconch morphology and/or shell microstrUcture are provided for Retiskenea statura (Goedert and Benham), Provanna antiqua Squires, Nucidana? aff. N. grasslei Allen, and Bathymodiolus willapaensis (Squires and Goedert). Modiolus (M.) willapaensis is placed within Bathymodiolus based on the elliptical-triangular shape of its juvenile shell, indicating that the divergence between vent/seep and whale/wood-fall inhabiting bathymodiolines took place at least 40 Ma. The first fossil species of the vent/seep genera Pyropetta (Pyropeltidae), Lurifiax (family uncertain), and Catillopecten? (Propeamussidae) are reported. Niso (Eulimidae), Xanthodaphne, Turrinosyrinx, Benthomangelia (Turridae), Ledella (Nuculanidae), Tindaria? (Tindariidae), and Delectopecten (Pectinidae) are reported lot the first time from fossil cold-seep assemblages. Larval developmental strategies are inferred from protoconch and prodissoconch morphologies in 14 species, which largely reflect the species' phylogenetic groups, as in modern vent and seep molluscs. The data presented here indicate that the radiation of toxoglossate turrids (Gastropoda) into deep water took place already in the Oligocene, and not in the Miocene as previously thought. Healed shell injuries and presumed naticid drill holes represent the oldest known fossil evidence of predation at cold-seeps. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Kiel, S (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM kiels@si.edu RI Kiel, Steffen/C-3150-2009 OI Kiel, Steffen/0000-0001-6281-100X NR 128 TC 61 Z9 62 U1 1 U2 6 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD JAN PY 2006 VL 80 IS 1 BP 121 EP 137 DI 10.1666/0022-3360(2006)080[0121:NRASOM]2.0.CO;2 PG 17 WC Paleontology SC Paleontology GA 997FV UT WOS:000234231500008 ER PT J AU Tong, JN Zhou, XJ Erwin, DH Zuo, JX Zhao, LS AF Tong, JN Zhou, XJ Erwin, DH Zuo, JX Zhao, LS TI Fossil fishes from the Lower Triassic of Majiashan, Chaohu, Anhui Province, China SO JOURNAL OF PALEONTOLOGY LA English DT Article AB The fossils described here were collected from the Lower Triassic (Olenekian) at two Majiashan sections in Chaohu City, Anhui Province, East China. Nine species belonging to five genera are introduced, including a new genus, Chaohuichthys, and some undetermined or unnamed fish specimens are discussed. The fish assemblage from Majiashan covers most of the Lower Triassic marine bony fish taxa known from China. C1 China Univ Geosci, GPMR & BGEG Labs, Wuhan 430074, Peoples R China. Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Tong, JN (reprint author), China Univ Geosci, GPMR & BGEG Labs, Wuhan 430074, Peoples R China. EM jntong@cug.edu.cn RI Erwin, Douglas/A-9668-2009 NR 37 TC 29 Z9 40 U1 1 U2 10 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 JAN PY 2006 VL 80 IS 1 BP 146 EP 161 DI 10.1666/0022-3360(2006)080[0146:FFFTLT]2.0.CO;2 PG 16 WC Paleontology SC Paleontology GA 997FV UT WOS:000234231500010 ER PT J AU Lyulin, OM Perevalov, VI Mandin, JY Dana, V Jacquemart, D Regalia-Jarlot, L Barbe, A AF Lyulin, OM Perevalov, VI Mandin, JY Dana, V Jacquemart, D Regalia-Jarlot, L Barbe, A TI Line intensities of acetylene in the 3-mu m region: New measurements of weak hot bands and global fitting SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE acetylene; infrared spectroscopy; vibro-rotational transitions; line intensities; transition dipole moment ID INTERNAL PARTITION SUMS; ENERGY-LEVELS; C2H2; MOLECULES; SPECTRUM; HITRAN AB About 170 line intensities of 14 weak parallel hot bands of acetylene have been measured in the 3-mu m region. Absolute values of line intensities are obtained with a mean uncertainty of 10%, except for a few lines of 3 very weak bands (Uncertainty Lip to 20%). Vibrational transition dipole moment and Herman-Wallis coefficients have been determined for each measured band. These measured line intensities together with previously published ones (JQSRT 2005;92:239-60) have been treated simultaneously within the framework of the effective operators approach. Using only 6 effective dipole moment parameters, it was possible to reproduce the 591 measured line intensities of the 20 bands with a root mean square of the residuals equal to 4.2%. (c) 2005 Elsevier Ltd. All rights reserved. C1 Russian Acad Sci, Lab Theoret Spect, Inst Atmospher Opt, Siberian Branch, Tomsk 634055, Russia. Univ Paris 06, CNRS, UMR 7092, Lab Phys Mol & Applicat, F-75252 Paris 05, France. Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, CNRS, UMR 6089, Grp Spectrometrie Mol & Atmospher,Fac Sci, F-51687 Reims 2, France. RP Perevalov, VI (reprint author), Russian Acad Sci, Lab Theoret Spect, Inst Atmospher Opt, Siberian Branch, 1,Akademicheskii Av, Tomsk 634055, Russia. EM vip@lts.iao.ru NR 17 TC 15 Z9 16 U1 0 U2 2 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 JAN PY 2006 VL 97 IS 1 BP 81 EP 98 DI 10.1016/j.jqsrt.2004.12.022 PG 18 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 995NG UT WOS:000234106400011 ER PT J AU MacIntyre, IG Aronson, RB AF MacIntyre, IG Aronson, RB TI Lithified and unlithified MG-calcite precipitates in tropical reef environments SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID CARIBBEAN FRINGING REEF; GREAT BARRIER-REEF; SUBMARINE LITHIFICATION; CARBONATE MUD; GEOLOGICAL RECORD; BRITISH-HONDURAS; GALETA POINT; RED-SEA; BELIZE; CEMENTATION AB Push cores from the branching-coral framework of lagoonal reefs in Belize and Panama indicate that the micritic Mg-calcite in the unlithified mud matrix is similar in composition to the well documented submarine lithified micritic crusts and infillings found in open reef framework. The sediment matrix of the lagoonal framework contains significant concentrations of 12 to 13 mole % MgCO3 calcite that shows almost no signs of skeletal origins, as indicated by a fairly consistent mineralogy and independent distribution patterns in sand-, silt-, and clay-size fractions. Its sedimentological and mineralogical similarity to cemented micritic crusts and infillings suggests that the precipitation of micritic Mg-calcite is widespread in tropical-reef waters and becomes lithified when precipitated in open frameworks but remains unlithified when trapped in impermeable lagoonal muddy sediments. C1 Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA. Univ S Alabama, Dept Marine Sci, Mobile, AL 36688 USA. RP MacIntyre, IG (reprint author), Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. EM macintyr@si.edu NR 69 TC 18 Z9 20 U1 0 U2 6 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 J9 J SEDIMENT RES JI J. Sediment. Res. PD JAN-FEB PY 2006 VL 76 IS 1-2 BP 81 EP 90 DI 10.2110/jsr.2006.05 PG 10 WC Geology SC Geology GA 018EM UT WOS:000235746800007 ER PT J AU Connor, R AF Connor, R TI 50th anniversary perspectives on the American helicopter industry SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB In the fifty years following the first issue of the Journal of the American Helicopter Society, the rotary-wing industry has seen moments of great technological and operational success, as well as struggles and disappointments. As that first issue was published, the industry was beginning to mature and was experiencing what might be regarded as a "Golden Age," much as fixed-wing aviation had experienced in the inter-war years where enthusiasm ran high and public and private sector investment was in abundance. However, the path to maturity was far different for the rotary-wing industry than it had been in the fixed-wing sector. The paper contextualizes the innovations in rotary-wing flight against the military, political, economic and cultural landscape that alternatively restricted and encouraged the growth of this particularly challenging sector of the aerospace industry. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Connor, R (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 53 TC 0 Z9 0 U1 0 U2 0 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JAN PY 2006 VL 51 IS 1 BP 22 EP 42 PG 21 WC Engineering, Aerospace SC Engineering GA 016CC UT WOS:000235597200003 ER PT J AU Eberhard, WG AF Eberhard, WG TI Sexually reversed copulatory courtship roles and possible nuptial feeding in the soldier beetle Ditemnus acantholabus (Champion 1915) (Coleoptera : Cantharidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE copulatory courtship; sexual selection; Ditemnus; Cantharidae ID CRYPTIC FEMALE CHOICE; BEHAVIOR; INSECTS AB Male courtship during copulation is common in insects and spiders, and presumably serves to induce the female to fertilize her eggs with the male's sperm. Fragmentary observations indicate that in Ditemnus acantholobus, typical male and female roles are reversed. The female courts vigorously and persistently during copulation while keeping one portion of the male's highly modified pronotum inside her buccal cavity. I propose that female copulatory courtship in this species functions to induce the male to provide material from his pronotum for the female to ingest, and that the species-specific modifications of the male pronotum are courtship devices. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM archisepsis@biologia.ucr.ac.cr NR 21 TC 4 Z9 4 U1 3 U2 10 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JAN PY 2006 VL 79 IS 1 BP 13 EP 22 DI 10.2317/0501.20.1 PG 10 WC Entomology SC Entomology GA 016CW UT WOS:000235599300002 ER PT J AU DiMichele, WA Phillips, TL Pfefferkorn, HW AF DiMichele, William A. Phillips, Tom L. Pfefferkorn, Hermann W. TI Paleoecology of Late Paleozoic pteridosperms from tropical Euramerica SO JOURNAL OF THE TORREY BOTANICAL SOCIETY LA English DT Review DE Carboniferous; Devonian; paleoecology; Paleozoic; Permian; pteridosperms; seed ferns ID EARLY SEED PLANTS; COAL-SWAMP VEGETATION; NORTH-CENTRAL TEXAS; CENTRAL NEW-MEXICO; GROWTH HABIT; PERMIAN PALEOBOTANY; MEDULLOSAN PTERIDOSPERMS; DINANTIAN FLORAS; ILLINOIS-BASIN; FOSSIL PLANTS AB DIMICHELE, W. A. (Department of Paleobiology, NMNH, Smithsonian Institution, Washington, DC 20560), T L. PHILLIPS (Department of Plant Biology, University of Illinois, Urbana, IL 61801), AND H. W. PFEFFERKORN (Department of Earth and Environmental Science, University of Pennsylvania, Philadelphia, PA 19106). Paleoecology of Late Paleozoic pteridosperms from tropical Euramerica. J. Torrey Bot. Soc. 133: 83-118. 2006-Late Paleozoic pteridosperms are a paraphyletic group of seed plants that were prominent elements of tropical ecosystems, primarily those of wetlands or the wetter portions of seasonally dry environments. Because the group is more a tradition-based, historical construct than a well circumscribed phylogenetic lineage, the wide variance in ecological roles and ecomorphological attributes should not be surprising. Pteridosperms can be the dominant canopy trees in local habitats, prominent understory trees, scrambling ground cover, thicket-formers, or hana-like plants and vines. Some species appear to have been weedy opportunists, although this ecological strategy seems to be a minor part of the wide spectrum of pteridosperm life habits. Most pteridosperms appear to have preferred wetter parts of the landscape, though not standing water, and relatively nutrient-rich settings (in comparison with groups such as tree ferns or lycopsids). Of the Paleozoic pteridosperms as traditionally circumscribed, only the peltasperms survived to become major elements in the Mesozoic. However, these plants may have been part of a derived seed-plant clade that also includes the corystosperms and cycads (see Hilton and Bateman, this volume), indicating that only the most derived of the Pateozoic pteridosperm lineages, those that appear to have evolved initially in extrabasinal settings, persisted into the Mesozoic. C1 Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19106 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, NMNH, Dept Paleobiol, Washington, DC 20560 USA. EM dimichele@si.edu RI DiMichele, William/K-4301-2012 NR 263 TC 57 Z9 60 U1 1 U2 8 PU TORREY BOTANICAL SOC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1095-5674 J9 J TORREY BOT SOC JI J. Torrey Bot. Soc. PD JAN-MAR PY 2006 VL 133 IS 1 BP 83 EP 118 DI 10.3159/1095-5674(2006)133[83:POLPPF]2.0.CO;2 PG 36 WC Plant Sciences SC Plant Sciences GA 043ZV UT WOS:000237642600008 ER PT J AU Kalka, M Kalko, EKV AF Kalka, M Kalko, EKV TI Gleaning bats as underestimated predators of herbivorous insects: diet of Micronycteris microtis (Phyllostomidae) in Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Chiroptera; feeding rate; herbivory; infrared videotaping; insectivory; predation ID FORAGING STRATEGY; TROPICAL FORESTS; ARTHROPODS; BEHAVIOR; BIRDS; FOOD; PREFERENCES; RAINFALL; CANOPY; MYOTIS AB Predators of herbivorous insects play important roles in tropical ecosystems as herbivory may affect structure and diversity of plant populations. Although insectivorous bats are particularly abundant and diverse in the tropics, their impact on herbivorous insects is little understood. To assess prey consumption, we observed the gleaning bat Micronycteris microtis (Phyllostomidae) continuously for 3 mo including 16 full nights at a nightly feeding roost on Barro Colorado Island in Panama using infrared videotaping combined with collection of prey remains. Individual bats consumed about 61-84%, of their body mass in arthropods per night. Diet analysis revealed a high percentage of herbivorous insects, constituting more than half (51'%) of all prey and over 70%) of prey biomass. Dominant prey were caterpillars (33%, of prey biomass), and other herbivores including crickets, kalydids, scarab beetles and phasmids. Furthermore, a novel feeding behaviour was observed as M. microtis selectively discarded parts of intestines of phytophagous insects before consumption, probably to avoid intake of plant material either for ballast reduction and/or for protection from secondary plant compounds. Combined with estimated feeding rates of insects in sympatric bat species, our data suggest that gleaning bats are important predators of herbivorous insects and might be underestimated reducers of herbivory in the tropics. C1 Univ Ulm, Dept Expt Ecol, D-89069 Ulm, Germany. Free Univ Berlin, Dept Zool, D-14195 Berlin, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Kalka, M (reprint author), Univ Ulm, Dept Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM Elisabeth.Kalko@uni-ulm.de NR 53 TC 44 Z9 45 U1 0 U2 23 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2006 VL 22 BP 1 EP 10 DI 10.1017/S0266467405002920 PN 1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 004GT UT WOS:000234740700001 ER PT J AU King, DA Wright, SJ Connell, JH AF King, DA Wright, SJ Connell, JH TI The contribution of interspecific variation in maximum tree height to tropical and temperate diversity SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Australia; biodiversity; forest architecture hypothesis; forest stratification; Panama; temperate forest; tree height; tropical forest; USA ID MIXED MESOPHYTIC FOREST; RAIN-FOREST; NEOTROPICAL FOREST; SPECIES-DIVERSITY; CANOPY STRUCTURE; DEPENDENT RECRUITMENT; SIZE DISTRIBUTIONS; ASYMPTOTIC HEIGHT; SHADE TOLERANCE; BARRO-COLORADO AB Maximum height was assessed for tree species from seven temperate deciduous forests, one subtropical forest and one tropical forest and combined with published tree heights for three other tropical forests. The temperate deciduous forests showed a strong concentration of canopy species and a dearth of subcanopy species. In contrast. the four tropical forests showed more uniform distributions of maximum heights, while the subtropical forest had an intermediate distribution. The tropical and subtropical sites had greater densities of small trees than did the temperate sites and most of these small trees were members of small- to medium-sized species. Sapling recruitment per unit stem basal area increased with declining maximum height in Panama, which is consistent with the criterion for coexistence of species of differing stature derived from Kohyama's forest architecture hypothesis. Greater penetration of light into gaps and favourable conditions for growth over most of the year may allow more smaller-statured species to coexist with canopy trees in tropical vs. temperate forests. C1 Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP King, DA (reprint author), Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, 22 Divin Ave, Cambridge, MA 02138 USA. EM dkingaz@yahoo.com RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 65 TC 47 Z9 56 U1 2 U2 33 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 JAN PY 2006 VL 22 BP 11 EP 24 DI 10.1017/S0266467405002774 PN 1 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 004GT UT WOS:000234740700002 ER PT J AU Davies, SJ Semui, H AF Davies, SJ Semui, H TI Competitive dominance in a secondary successional rain-forest community in Borneo SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE competition; Dillenia suffruticosa; Duabanya moluccana; Ficus grossularioides; Melastoma malabathricum; Nauclea maingayi; nutrient limitation; pioneer trees; succession; tree seedlings; Trema cannabina; tropical forest; Vitex pubescens ID MELASTOMA-MALABATHRICUM L; DIPTEROCARP SEEDLINGS; ADINANDRA BELUKAR; PLANT SUCCESSION; EASTERN AMAZONIA; TROPICAL FOREST; SINGAPORE; RESPONSES; PATTERNS; ALUMINUM AB Competitive interactions among pioneer species may have a significant impact on the course of secondary succession in tropical rain forests. We predicted that the outcome of competitive interactions in early succession would vary with soil nutrient availability. To test this hypothesis we grew seven pioneer tree species alone and in dense competitive mixtures, with four nutrient treatments: no nutrient addition, and N, P, and N plus P addition. Performance of plants grown alone and in mixtures was strongly nutrient limited. However, contrary to expectation, the competitive hierarchy among the seven species was almost identical among the four nutrient treatments. The dominant species, Melastoma malabathricum, accounted for > 70% of total stand biomass in all nutrient treatments. Seedlings of this species had higher rates of gas exchange and initial growth, and lower root allocation than the other species. Profiles of light availability within the competitive stands indicated that light levels at ground level were well above levels at which pioneer species can successfully survive and grow, yet seedlings of species other than Melastoma remained stunted. Leaf N concentrations in all stands were 25-55% reduced by competitive interactions, and N addition increased relative competitive performance in only Melastoma suggesting that Melastoma was particularly effective at N acquisition, limiting nutrient uptake by the other species. Toward the end of the experiment individuals of Melastoma began to reproduce, suggesting that the competitive hierarchy would have changed in a longer-duration experiment. C1 Harvard Univ, Ctr Trop Forest Serv, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. Univ Malaysia Sarawak, Inst Biodiver & Environm Conservat, Kota Samarahan, Sarawak, Malaysia. RP Davies, SJ (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. EM sdavies@oeb.harvard.edu NR 34 TC 9 Z9 11 U1 1 U2 13 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 JAN PY 2006 VL 22 BP 53 EP 64 DI 10.1017/S0266767405002944 PN 1 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 004GT UT WOS:000234740700006 ER PT J AU Riley, S AF Riley, S TI The Ernesto "Che" Guevara school for Wayward girls. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Publ Libs, Washington, DC 20560 USA. RP Riley, S (reprint author), Smithsonian Inst, Publ Libs, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 JAN PY 2006 VL 131 IS 1 BP 95 EP 95 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 003GW UT WOS:000234670800072 ER PT J AU Herwig, RP Cordell, JR Perrins, JC Dinnel, PA Gensemer, RW Stubblefield, WA Ruiz, GM Kopp, JA House, ML Cooper, WJ AF Herwig, Russell P. Cordell, Jeffery R. Perrins, Jake C. Dinnel, Paul A. Gensemer, Robert W. Stubblefield, William A. Ruiz, Gregory M. Kopp, Joel A. House, Marcia L. Cooper, William J. TI Ozone treatment of ballast water on the oil tanker S/T Tonsina: chemistry, biology and toxicity SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE aquatic nuisance species; non-indigenous species; ballast water; ozone treatment; bromine; total residual oxidant ID MINNOWS CYPRINODON-VARIEGATUS; SAN-FRANCISCO BAY; BROMATE FORMATION; DRINKING-WATER; NATURAL-POPULATIONS; MARINE COMMUNITIES; ADVANCED OXIDATION; PRODUCT FORMATION; TREATMENT SYSTEM; RISK-ASSESSMENT AB Worldwide transfer and introduction of non-indigenous species in ballast water causes significant environmental and economic impact. One way to address this problem is to remove or inactivate organisms that are found in ballast water. In this study, 3 experiments were conducted in Puget Sound, Washington, USA, using a prototype ozone treatment system installed on a commercial oil tanker, the S/T Tonsina. Treatment consisted of ozone gas diffused into a ballast tank for 5 and 10 h. Treatment and control tanks were sampled during the ozonation period for chemistry, culturable bacteria, phytoplankton and zooplankton. Selected fish and invertebrates were placed in cages deployed in the treatment and control tanks. Ozone introduced into seawater rapidly converts bromide (Br-) to bromines (HOBr/OBr-), compounds that are disinfectants. These were measured as total residual oxidant (TRO). Ozone treatment inactivated large portions of culturable bacteria, phytoplankton and zooplankton. The highest reductions observed were 99.99% for the culturable bacteria, > 99% for dinoflagellates and 96% for zooplankton. Caged animal results varied among taxa and locations in the ballast tank. Sheepshead minnows and mysid shrimp were most susceptible, shore crabs and amphipods the least. Distribution of ozone in the treatment tank was not homogenous during experiments, as suggested by the observed TRO concentrations and lower efficacies for inactivating the different taxa in selected ballast tank locations. Low concentrations of bromoform, a disinfection byproduct, were found in treated ballast water. C1 Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. ENSR Int, Ft Collins, CO 80521 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. Petrotech Resources Alaska, Anchorage, AK 99510 USA. Univ N Carolina, Dept Chem, Wilmington, NC 28409 USA. Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28409 USA. RP Herwig, RP (reprint author), Univ Washington, Sch Aquat & Fishery Sci, Box 355020, Seattle, WA 98195 USA. EM herwig@u.washington.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 67 TC 27 Z9 28 U1 1 U2 20 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2006 VL 324 BP 37 EP 55 DI 10.3354/meps324037 PG 19 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 110KE UT WOS:000242376800003 ER PT J AU Kuffner, IB Walters, LJ Becerro, MA Paul, VJ Ritson-Williams, R Beach, KS AF Kuffner, Ilsa B. Walters, Linda J. Becerro, Mikel A. Paul, Valerie J. Ritson-Williams, Raphael Beach, Kevin S. TI Inhibition of coral recruitment by macroalgae and cyanobacteria SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE allelopathy; coral-algae interactions; Dictyota spp.; Lyngbya spp.; phase shift ID BENTHIC CYANOBACTERIA; SCLERACTINIAN CORAL; POCILLOPORA-DAMICORNIS; LARVAL METAMORPHOSIS; NUTRIENT ENRICHMENT; JUVENILE CORALS; CLIMATE-CHANGE; ALGAL BIOMASS; DICTYOTA SPP.; PHASE-SHIFTS AB Coral recruitment, is a key process in the maintenance and recovery of coral reef ecosystems. While intense competition between coral and algae is often assumed on reefs that have undergone phase shifts from coral to algal dominance, data examining the competitive interactions involved, particularly during the larval and immediate post-settlement stage, are scarce. Using a series of field and outdoor seawater table experiments, we tested the hypothesis that common species of macroalgae and cyanobacteria inhibit coral recruitment. We examined the effects of Lyngbya spp., Dictyota spp., Lobophora variegata (J. V. Lamouroux) Womersley, and Chondrophycus poiteaui (J. V. Lamouroux) Nam (formerly Laurencia poiteaui) on the recruitment success of Porites astreoides larvae. All species but C. poiteaui caused either recruitment inhibition or avoidance behavior in P. astreoides larvae, while L. confervoides and D. menstrualis significantly increased mortality rates of P. astreoides recruits. We also tested the effect of some of these macrophytes on larvae of the gorgonian octocoral Briareum asbestinum. Exposure to Lyngbya majuscula reduced survival and recruitment in the octocoral larvae. Our results provide evidence that algae and cyanobacteria use tactics beyond space occupation to inhibit coral recruitment. On reefs experiencing phase shifts or temporary algal blooms, the restocking of adult coral populations may be slowed due to recruitment inhibition, thereby perpetuating reduced coral cover and limiting coral community recovery. C1 US Geol Survey, Ctr Coastal & Watershed Studies, St Petersburg, FL 33701 USA. Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Univ Tampa, Dept Biol, Tampa, FL 33606 USA. RP Kuffner, IB (reprint author), US Geol Survey, Ctr Coastal & Watershed Studies, 600 4th St S, St Petersburg, FL 33701 USA. EM ikuffner@usgs.gov RI Becerro, Mikel/A-5325-2008; Kuffner, Ilsa/A-6416-2008; OI Kuffner, Ilsa/0000-0001-8804-7847; Becerro, Mikel/0000-0002-6047-350X NR 55 TC 146 Z9 154 U1 11 U2 85 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2006 VL 323 BP 107 EP 117 DI 10.3354/meps323107 PG 11 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 103XY UT WOS:000241921700010 ER PT J AU Kline, DI Kuntz, NM Breitbart, M Knowlton, N Rohwer, F AF Kline, David I. Kuntz, Neilan M. Breitbart, Mya Knowlton, Nancy Rohwer, Forest TI Role of elevated organic carbon levels and microbial activity in coral mortality SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE coral reef decline; dissolved organic carbon; coral; Montastraea; bacteria; Caribbean; nutrients ID NUTRIENT ENRICHMENT; BARRIER-REEF; MUCUS; COMMUNITIES; DIVERSITY; DISEASE; ECOSYSTEM; BACTERIA; PACIFIC; IMPACTS AB Coral reefs are suffering a long-term global decline, yet the causes remain contentious. The role of poor water quality in this decline is particularly unclear, with most previous studies providing only weak correlations between elevated nutrient levels and coral mortality. Here we experimentally show that routinely measured components of water quality (nitrate, phosphate, ammonia) do not cause substantial coral mortality. In contrast, dissolved organic carbon (DOC), which is rarely measured on reefs, does. Elevated DOC levels also accelerate the growth rate of microbes living in the corals' surface mucopolysaccharide layer by an order of magnitude, suggesting that mortality occurs due to a disruption of the balance between the coral and its associated microbiota. We propose a model by which elevated DOC levels cause Caribbean reefs to shift further from coral to macroalgal dominance. Increasing DOC levels on coral reefs should be recognized as a threat and routinely monitored. C1 San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. Univ Calif San Diego, Ctr Marine Biodivers & Conservat, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Balboa, Panama. San Diego State Univ, Ctr Microbial Sci, San Diego, CA 92182 USA. RP Rohwer, F (reprint author), San Diego State Univ, Dept Biol, LS301,5500 Campanile Dr, San Diego, CA 92182 USA. EM frohwer@sunstroke.sdsu.edu RI Breitbart, Mya/B-1366-2009 OI Breitbart, Mya/0000-0003-3210-2899 NR 45 TC 127 Z9 133 U1 1 U2 34 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2006 VL 314 BP 119 EP 125 DI 10.3354/meps314119 PG 7 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 060YG UT WOS:000238837500011 ER PT J AU Guan, Y Huss, GR Leshin, LA MacPherson, GJ McKeegan, KD AF Guan, Y Huss, GR Leshin, LA MacPherson, GJ McKeegan, KD TI Oxygen isotope and Al-26-Mg-26 systematics of aluminum-rich chondrules from unequilibrated enstatite chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Chondrites and the Protoplanetary Disk CY NOV, 2004 CL Kaua i, HI ID EARLY SOLAR-SYSTEM; CARBONACEOUS CHONDRITES; FERROMAGNESIAN CHONDRULES; INCLUSIONS; AL-26; NEBULA; ABUNDANCES; HETEROGENEITY; CONSTRAINTS; ANORTHITE AB Correlated in situ analyses of the oxygen and magnesium isotopic compositions of aluminurn-rich chondrules from unequilibrated enstatite chondrites were obtained using an ion microprobe. Among eleven aluminum-rich chondrules and two plagioclase fragments measured for Al-26-Mg-16 systematics, only one aluminum-rich chondrule contains excess Mg-26 from the in situ decay of Al-26; the inferred initial ratio (Al-26/Al-27)(0) = (6.8 +/- 2.4) x 10(-6) is consistent with ratios observed in chondrules from carbonaceous chondrites and unequilibrated ordinary chondrites. The oxygen isotopic compositions of five aluminum-rich chondrules and one plagioclase fragment define a line of slope similar to 0.6 +/- 0.1 on a three-oxygen-isotope diagram, overlapping the field defined by ferromagnesian chondrules in enstatite chondrites but extending to more O-16-rich compositions with a range in delta O-18 of about similar to 12 parts per thousand. Based on their oxygen isotopic compositions, aluminum-rich chondrules in unequilibrated enstatite chondrites are probably genetically related to ferromagnesian chondrules and are not simple mixtures of materials from ferromagnesian chondrules and calcium-aluminum-rich inclusions (CAIs). Relative to their counterparts from unequilibrated ordinary chondrites, aluminum-rich chondrules from unequilibrated enstatite chondrites show a narrower oxygen isotopic range and much less resolvable excess Mg-26 from the in situ decay of Al-26, probably resulting from higher degrees of equilibration and isotopic exchange during post-crystallization metamorphism. However, the presence of Al-26-bearing chondrules within the primitive ordinary, carbonaceous, and now enstatite chondrites suggests that Al-26 was at least approximately homogeneously distributed across the chondrite-forming region. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Guan, Y (reprint author), Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. EM yunbin.guan@asu.edu RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011 OI McKeegan, Kevin/0000-0002-1827-729X; NR 40 TC 12 Z9 13 U1 0 U2 1 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 JAN PY 2006 VL 41 IS 1 BP 33 EP 47 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 020OO UT WOS:000235919400004 ER PT J AU Georgescu, MD Braun, WK AF Georgescu, Marius Dan Braun, Willi Klaus TI Jurassic and Cretaceous charophyta of Western Canada SO MICROPALEONTOLOGY LA English DT Article AB Jurassic and Cretaceous charophytes of Western Canada (Saskatchewan and Alberta) are known from two narrow stratigraphic intervals and parts of the Bathonian (Middle Jurassic) and Aptian (Early Cretaceous) sequences of the prairie sequences. Thirteen species are accounted for with, twelve from the Bathonian and three from the Aptian. The Bathonian assemblage is one of the richest worldwide, and it provides valuable insight on the earliest phase of the Jurassic-Early Cretaceous radiation of the group. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. RP Georgescu, MD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, 10 & Constitut Ave, Washington, DC 20013 USA. EM georgescum@si.edu NR 31 TC 0 Z9 0 U1 1 U2 2 PU MICROPALEONTOLOGY PRESS PI NEW YORK PA AMER MUSEUM NAT HISTORY 79TH ST AT CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0026-2803 J9 MICROPALEONTOLOGY JI Micropaleontology PY 2006 VL 52 IS 4 BP 357 EP 369 DI 10.2113/gsmicropal.52.4.357 PG 13 WC Paleontology SC Paleontology GA 101TF UT WOS:000241762800004 ER PT J AU Topf, AL Gilbert, MTP Dumbacher, JP Hoelzel, AR AF Topf, AL Gilbert, MTP Dumbacher, JP Hoelzel, AR TI Tracing the phylogeography of human populations in Britain based on 4th-11th century mtDNA genotypes SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE ancient DNA; Doggerland; human; phylogeography ID BRITISH-ISLES; DNA-SEQUENCES; ANCIENT DNA; EUROPE; EVOLUTION; ORIGIN; POOL AB Some of the transitional periods of Britain during the first millennium A.D. are traditionally associated with the movement of people from continental Europe, composed largely of invading armies (e.g., the Roman, Saxon, and Viking invasions). However, the extent to which these were migrations (as opposed to cultural exchange) remains controversial. We investigated the history of migration by women by amplifying mitochondrial DNA (mtDNA) from ancient Britons who lived between approximately A.D. 300-1,000 and compared these with 3,549 modern mtDNA database genotypes from England, Europe, and the Middle East. The objective was to assess the dynamics of the historical population composition by comparing genotypes in a temporal context. Towards this objective we test and calibrate the use of rho statistics to identify relationships between founder and source populations. We find evidence for shared ancestry between the earliest sites (predating Viking invasions) with modern populations across the north of Europe from Norway to Estonia, possibly reflecting common ancestors dating back to the last glacial epoch. This is in contrast with a late Saxon site in Norwich, where the genetic signature is consistent with more recent immigrations from the south, possibly as part of the Saxon invasions. C1 Univ Durham, Sch Biol & Biomed Sci, Durham, England. Univ Oxford, Dept Zool, Ancient Biomol Ctr, Oxford OX1 3PS, England. Natl Museum Nat Hist, Smithsonian Inst, Genet Program, Washington, DC 20560 USA. RP Hoelzel, AR (reprint author), Univ Durham, Sch Biol & Biomed Sci, Durham, England. EM a.r.hoelzel@dur.ac.uk RI Gilbert, Marcus/A-8936-2013 OI Gilbert, Marcus/0000-0002-5805-7195 NR 57 TC 19 Z9 20 U1 3 U2 15 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 JAN PY 2006 VL 23 IS 1 BP 152 EP 161 DI 10.1093/molbev/msj013 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 991WA UT WOS:000233843900018 PM 16151183 ER PT J AU Hawley, DM Hanley, D Dhondt, AA Lovette, IJ AF Hawley, DM Hanley, D Dhondt, AA Lovette, IJ TI Molecular evidence for a founder effect in invasive house finch (Carpodacus mexicanus) populations experiencing an emergent disease epidemic SO MOLECULAR ECOLOGY LA English DT Article DE disease emergence; founder effect; genetic diversity; house finch; invasive species; microsatellite DNA; population bottleneck ID ENDANGERED GILA TOPMINNOW; EASTERN NORTH-AMERICA; ALLELE FREQUENCY DATA; MICROSATELLITE LOCI; GENETIC DIVERSITY; MYCOPLASMAL CONJUNCTIVITIS; NEW-ZEALAND; MUTATIONAL PROCESSES; F-STATISTICS; EVOLUTION AB The impact of founder events on levels of genetic variation in natural populations remains a topic of significant interest. Well-documented introductions provide a valuable opportunity to examine how founder events influence genetic diversity in invasive species. House finches (Carpodacus mexicanus) are passerine birds native to western North America, with the large eastern North American population derived from a small number of captive individuals released in the 1940s. Previous comparisons using amplified fragment length polymorphism (AFLP) markers found equivalent levels of diversity in eastern and western populations, suggesting that any genetic effects of the founder event were ameliorated by the rapid growth of the newly established population. We used an alternative marker system, 10 highly polymorphic microsatellites, to compare levels of genetic diversity between four native and five introduced house finch populations. In contrast to the AFLP comparisons, we found significantly lower allelic richness and heterozygosity in introduced populations across all loci. Three out of five introduced populations showed significant reductions in the ratio of the number of alleles to the allele size range, a within-population characteristic of recent bottlenecks. Finally, native and introduced populations showed significant pairwise differences in allele frequencies in every case, with stronger isolation by distance within the introduced than native range. Overall, our results provide compelling molecular evidence for a founder effect during the introduction of eastern house finches that reduced diversity levels at polymorphic microsatellite loci and may have contributed to the emergence of the Mycoplasma epidemic which recently swept the eastern range of this species. C1 Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. Ithaca Coll, Ornithol Lab, Ithaca, NY 14850 USA. RP Hawley, DM (reprint author), Smithsonian Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM dmh35@cornell.edu RI Dhondt, Andre/A-8292-2008; Hanley, Daniel/E-9484-2012; Hanley, Daniel/C-9080-2016; OI Hanley, Daniel/0000-0002-1646-4040; Hanley, Daniel/0000-0003-0523-4335; Hawley, Dana/0000-0001-9573-2914 NR 84 TC 65 Z9 68 U1 6 U2 31 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JAN PY 2006 VL 15 IS 1 BP 263 EP 275 DI 10.1111/j.1365-294X.2005.02767.x PG 13 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 994KD UT WOS:000234029800021 PM 16367845 ER PT J AU Furlanetto, SR McQuinn, M Hernquist, L AF Furlanetto, SR McQuinn, M Hernquist, L TI Characteristic scales during reionization SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : evolution; intergalactic medium; cosmology : theory ID DARK-MATTER HALOES; MICROWAVE BACKGROUND ANISOTROPIES; 21 CENTIMETER FLUCTUATIONS; PROBE WMAP OBSERVATIONS; GUNN-PETERSON TROUGH; EXCURSION SET MODEL; HIGH-REDSHIFT; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; NEUTRAL HYDROGEN AB One of the key observables of the reionization era is the distribution of neutral and ionized gas. Recently, Furlanetto, Zaldarriaga and Hernquist developed a simple analytic model to describe the growth of H II regions during this era. Here, we examine some of the fundamental simplifying assumptions behind this model and generalize it in several important ways. The model predicts that the ionized regions attain a well-defined characteristic size R-c that ranges from similar to 1 Mpc in the early phases to greater than or similar to 10 Mpc in the late phases. We show that R-c is determined primarily by the bias of the galaxies driving reionization; hence measurements of this scale constrain a fundamental property of the first galaxies. The variance around R-c, on the other hand, is determined primarily by the underlying matter power spectrum. We then show that increasing the ionizing efficiency of massive galaxies shifts R-c to significantly larger scales and decreases the importance of recombinations. These differences can be observed with forthcoming redshifted 21-cm surveys (increasing the brightness temperature fluctuations by up to a factor of 2 on large scales) and with measurements of small-scale anisotropies in the cosmic microwave background. Finally, we show that stochastic fluctuations in the galaxy population only broaden the bubble size distribution significantly if massive galaxies are responsible for most of the ionizing photons. We argue that the key results of this model are robust to many of our uncertainties about the reionization process. C1 CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Furlanetto, SR (reprint author), CALTECH, Div Phys Math & Astron, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu NR 78 TC 72 Z9 72 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2006 VL 365 IS 1 BP 115 EP 126 DI 10.1111/j.1365-2966.2005.09687.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VT UT WOS:000234853400014 ER PT J AU Baliunas, S Frick, P Moss, D Popova, E Sokoloff, D Soon, W AF Baliunas, S Frick, P Moss, D Popova, E Sokoloff, D Soon, W TI Anharmonic and standing dynamo waves: theory and observation of stellar magnetic activity SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : activity; stars : chromospheres; stars : late-type; stars : magnetic fields; stars : rotation ID MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; CHROMOSPHERIC ACTIVITY; DIFFERENTIAL ROTATION; DEPENDENCE; MODELS; AGE AB The familiar decadal cycle of solar activity is one expression of interannual variability of surface magnetism observed in stars on or near the lower main sequence. From studies of time-series of Ca II H and K emission fluxes that go back more than 35 yr and have been accumulated for such stars at the Mount Wilson Observatory by the HK Project, we define a quantitative measure, called anharmonicity, of the cyclic component of interannual magnetic variability. Anharmonicity provides a connection between observed variations in magnetic activity and the two-dimensional description of a Parker dynamo model. We explore the parameter space of the Parker dynamo model and find an excellent counterpart in the records of several of the lowest-mass (late K-type to early M-type) active stars in the HK Project sample to the solutions containing highly anharmonic, standing dynamo waves. We interpret anharmonicity apparent in the records as resulting from non-propagating or standing dynamo waves, which operate in a regime that is substantially supercriticial. There, for the majority of a cycle, or pulse of decadal-to-interdecadal variability, the large-scale magnetic fields are generated and maintained by winding of field by differential rotation rather than by the joint action of differential rotation and helical convection. Among the less active stars (the Sun is considered such a star in the HK Project sample) we find a correspondence between anharmonicity and Parker dynamo model solutions that include simple harmonic, migratory and/or intermediate-type dynamo wave patterns over a broad range of dynamo parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Continuous Media Mech, Perm 614061, Russia. Moscow MV Lomonosov State Univ, Dept Phys, Moscow 119992, Russia. Univ Manchester, Sch Math, Manchester M13 9PL, Lancs, England. RP Baliunas, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM moss@ma.man.ac.uk RI Frick, Peter/D-2345-2013 NR 30 TC 19 Z9 19 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 JAN 1 PY 2006 VL 365 IS 1 BP 181 EP 190 DI 10.1111/j.1365-2966.2005.09701.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VT UT WOS:000234853400022 ER PT J AU Barnes, AD Casares, J Charles, PA Clark, JS Cornelisse, R Knigge, C Steeghs, D AF Barnes, AD Casares, J Charles, PA Clark, JS Cornelisse, R Knigge, C Steeghs, D TI On the origin of the absorption features in SS 433 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; binaries : spectroscopic; stars : individual : SS 433; stars : winds, outflows ID SS 433; ACCRETION DISK; SS433; SPECTRUM; SYSTEM; STAR; PERIODS; MODEL AB We present high-resolution optical spectroscopy of the X-ray binary system SS 433, obtained over a wide range of orbital phases. The spectra display numerous weak absorption features, and include the clearest example seen to date of those features (resembling a mid-A type supergiant spectrum), which have previously been associated with the mass-donor star. However, the new data preclude the hypothesis that these features originate solely within the photosphere of the putative mass donor, indicating that there may be more than one region within the system producing an A supergiant-like spectrum, probably an accretion disc wind. Indeed, whilst we cannot confirm the possibility that the companion star is visible at certain phase combinations, it is possible that all supergiant-like features observed thus far are produced solely in a wind. We conclude that great care must be taken when interpreting the behaviour of these weak features. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Inst Astrofis Canarias, Tenerife 38200, Spain. S African Astron Observ, ZA-7935 Cape Town, South Africa. UCL, Dept Phys & Astron, London WC1E 6BT, England. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barnes, AD (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM adb@astro.soton.ac.uk RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 25 TC 17 Z9 17 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2006 VL 365 IS 1 BP 296 EP 302 DI 10.1111/j.1365-2966.2005.09725.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VT UT WOS:000234853400032 ER PT J AU Risaliti, G Maiolino, R Marconi, A Sani, E Berta, S Braito, V Ceca, RD Franceschini, A Salvati, M AF Risaliti, G Maiolino, R Marconi, A Sani, E Berta, S Braito, V Ceca, RD Franceschini, A Salvati, M TI Unveiling the nature of Ultraluminous Infrared Galaxies with 3-4 mu m spectroscopy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : active; galaxies : starburst; infrared : galaxies ID POLYCYCLIC AROMATIC-HYDROCARBONS; DIFFUSE INTERSTELLAR-MEDIUM; ACTIVE GALACTIC NUCLEUS; SPITZER-SPACE-TELESCOPE; BROAD-LINE REGIONS; SEYFERT 2 GALAXIES; XMM-NEWTON; OPTICAL SPECTROSCOPY; ABSORPTION FEATURE; EMISSION AB We present the results of L-band spectroscopical observations of local bright Ultraluminous Infrared Galaxies (ULIRGs), performed with the Infrared Spectrometer And Array Camera (ISAAC) at the Very Large Telescope. The excellent sensitivity of the telescope and of the instrument provided spectra of unprecedented quality for this class of objects, which allowed a detailed study of the active galactic nucleus (AGN)/starburst contribution to the energy output, and of the composition of the circumnuclear absorber. We discuss the L-band spectral features of seven single sources, and the statistical properties of a complete sample of 15 sources obtained combining our observations with other published 3-4 mu m spectra. Our main results are as follows. (i) When a spectral indicator suggesting the presence of an AGN (low equivalent width of the 3.3-mu m emission line, steep lambda-f(lambda) spectrum, presence of an absorption feature at 3.4 mu m) is found, the AGN is always confirmed by independent analysis at other wavelengths. Conversely, in all known AGNs at least one of the above indicators is present. (ii) Two new diagnostic diagrams are proposed combining the above indicators, in which starbursts and AGNs are clearly and completely separated. (iii) The above diagnostic techniques are possible with spectra of relatively low quality, which can be obtained for several tens of ULIRGs with currently available telescopes. This makes L-band spectroscopy the current best tool to disentangle AGN and starburst contributions in ULIRGs. (iv) The L-band properties of ULIRGs are heterogeneous. However, we show that all the spectral differences among ULIRGs can be reproduced starting from pure intrinsic AGN and starburst spectra and two varying parameters: the amount of dust extinction of the AGN component, and the relative AGN/starburst contribution to the bolometric luminosity. (v) Using the above decomposition model, we show that AGNs in ULIRGs have a low dust-to-gas ratio and a dust extinction curve different from Galactic. (vi) The estimate of the presence and contribution of AGNs in a complete sample shows that AGNs are hosted by approximately two-thirds of ULIRGs, but their energetic contribution is relevant (> 30 per cent of the bolometric luminosity) only in similar to 20 per cent of the sample. C1 Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. INAF, Osservatorio Astron Brera, Milan, Italy. RP Risaliti, G (reprint author), Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy. EM risaliti@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X; Della Ceca, Roberto/0000-0001-7551-2252 NR 57 TC 62 Z9 62 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2006 VL 365 IS 1 BP 303 EP 320 DI 10.1111/j.1365-2966.2005.09715.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 005VT UT WOS:000234853400033 ER PT J AU Volkert, J AF Volkert, J TI The 'rescue artist': A true story of art, thieves, and the hunt for a missing masterpiece. SO MUSEUM NEWS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Volkert, J (reprint author), Smithsonian Inst, Natl Museum Amer Indian, 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 JAN-FEB PY 2006 VL 85 IS 1 BP 25 EP + PG 3 WC Art SC Art GA 044ZN UT WOS:000237712500009 ER PT J AU Paul, VJ Puglisi, MP Ritson-Williams, R AF Paul, VJ Puglisi, MP Ritson-Williams, R TI Marine chemical ecology SO NATURAL PRODUCT REPORTS LA English DT Review ID BARNACLE BALANUS-AMPHITRITE; POLYCHAETE HYDROIDS-ELEGANS; ALGA FUCUS-VESICULOSUS; CORAL-REEF FISH; BIFURCARIA-BIFURCATA CYSTOSEIRACEAE; URCHIN HOLOPNEUSTES-PURPURASCENS; WOUND-ACTIVATED TRANSFORMATION; CALLINECTES-SAPIDUS MEGALOPAE; WESTERN ANTARCTIC PENINSULA; NATURAL PLANKTON COMMUNITY AB This review covers the recent marine chemical ecology literature for phytoplankton, macroalgae, sponges and other benthic invertebrates; 249 references are cited. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. NR 249 TC 95 Z9 105 U1 1 U2 22 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0265-0568 J9 NAT PROD REP JI Nat. Prod. Rep. PY 2006 VL 23 IS 2 BP 153 EP 180 DI 10.1039/b404735b PG 28 WC Biochemistry & Molecular Biology; Chemistry, Medicinal; Chemistry, Organic SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy; Chemistry GA 027AW UT WOS:000236386400002 PM 16572226 ER PT J AU Stoner, R Walsworth, R AF Stoner, R Walsworth, R TI Atomic physicS - Collisions give sense of direction SO NATURE PHYSICS LA English DT News Item AB The ability to measure small or slow rotations relative to an inertial frame is valuable in navigation as well as in fundamental physics. A device that exploits techniques developed in atomic physics could lead to sensitive and compact rotation sensors. C1 Draper Labs, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stoner, R (reprint author), Draper Labs, Cambridge, MA 02139 USA. EM rstoner@draper.com; rwalsworth@cfa.harvard.edu OI Stoner, Richard/0000-0001-7949-6747 NR 9 TC 8 Z9 8 U1 1 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD JAN PY 2006 VL 2 IS 1 BP 17 EP 18 DI 10.1038/nphys204 PG 2 WC Physics, Multidisciplinary SC Physics GA 007HF UT WOS:000234958900013 ER PT J AU Weldon, PJ Cranmore, CF Chatfield, JA AF Weldon, PJ Cranmore, CF Chatfield, JA TI Prey-rolling behavior of coatis (Nasua spp.) is elicited by benzoquinones from millipedes SO NATURWISSENSCHAFTEN LA English DT Article ID DIET AB Coatis (Nasua spp.), gregarious, omnivorous carnivores that range in forests from the southwestern USA to south America, dispatch millipedes by rolling them on the ground using rapid, alternating movements of their forepaws. Prey rolling of millipedes is thought to stimulate the depletion of their defensive secretions and to wipe off secretions before millipedes are consumed. We report that prey-rolling behavior in Nasua spp. is elicited by 1,4-benzoquinone; 2-methyl-1,4-benzoquinone; and 2-methoxy-3-methyl-1,4-benzoquinone, the chief components of the defensive secretions of julidan, spirobolidan, and spirostreptidan millipedes. Chemicals elaborated for defense sometimes evolutionarily "backfire," providing cues to predators on the presence or identity of prey. The elicitation of prey-rolling behavior in Nasua spp. by benzoquinones illustrates this effect for millipedes (and possibly other arthropods) that defensively discharge these compounds. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Tri Lakes Vet Clin & Exot, Mt Pleasant, TX 75455 USA. RP Chatfield, JA (reprint author), Gladys Porter Zoo, 500 Ringgold St, Brownsville, TX 78520 USA. EM jchatfield@gpz.org NR 16 TC 5 Z9 5 U1 1 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JAN PY 2006 VL 93 IS 1 BP 14 EP 16 DI 10.1007/s00114-005-0064-z PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 006DL UT WOS:000234875600002 PM 16391932 ER PT J AU Fernandez-Marin, H Zimmerman, JK Wcislo, WT AF Fernandez-Marin, H Zimmerman, JK Wcislo, WT TI Acanthopria and Mimopriella parasitoid wasps (Diapriidae) attack Cyphomyrmex fungus-growing ants (Formicidae, Attini) SO NATURWISSENSCHAFTEN LA English DT Article ID HYMENOPTERA; PREDATION; DEFENSE AB New World diapriine wasps are abundant and diverse, but the biology of most species is unknown. We provide the first description of the biology of diapriine wasps, Acanthopria spp. and Mimopriella sp., which attack the larvae of Cyphomyrmex fungus-growing ants. In Puerto Rico, the koinobiont parasitoids Acanthopria attack Cyphomyrmex minutus, while in Panama at least four morphospecies of Acanthopria and one of Mimopriella attack Cyphomyrmex rimosus. Of the total larvae per colony, 0-100% were parasitized, and 27-70% of the colonies per population were parasitized. Parasitism rate and colony size were negatively correlated for C. rimosus but not for C. minutus. Worker ants grasped at, bit, and in some cases, killed adult wasps that emerged in artificial nests or tried to enter natural nests. Parasitoid secondary sex ratios were female-biased for eclosing wasps, while field collections showed a male-biased sex ratio. Based on their abundance and success in attacking host ants, these minute wasps present excellent opportunities to explore how natural enemies impact ant colony demography and population biology. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Puerto Rico, Dept Biol, Puerto Real 00931, Spain. Univ Puerto Rico, Inst Studies Trop Ecosyst, San Juan, PR 00936 USA. RP Fernandez-Marin, H (reprint author), Smithsonian Trop Res Inst, Apdo 0843-03092, Balboa, Panama. EM ic972735@rrpac.upr.clu.edu; WcisloW@si.edu NR 15 TC 11 Z9 11 U1 1 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JAN PY 2006 VL 93 IS 1 BP 17 EP 21 DI 10.1007/s00114-005-0048-z PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 006DL UT WOS:000234875600003 PM 16315027 ER PT J AU Miljutin, DM Tchesunov, AV Hope, WD AF Miljutin, DM Tchesunov, AV Hope, WD TI Rhaptothyreus typicus Hope & Murphy, 1969 (Nematoda : Rhaptothyreidae): an anatomical study of an unusual deep-sea nematode SO NEMATOLOGY LA English DT Article DE amphid; anatomy; Atlantic Ocean; marine nematodes; morphology; morphometrics; SEM; symbiotic intracellular bacteria; TEM; trophosome; ultrastructure ID BENTHIMERMITHIDAE; PETTER AB Descriptions are given for the males of Rhaptothyreus typicus, a morphologically unique and incompletely investigated deep-sea nematode, using light microscopy, TEM, and SEM. The cephalic sensilla are arranged in two circles: an anterior circle consisting of six pairs of papilliform sensilla and a posterior circle consisting of four papilliform sensilla. The fovea of the giant, oblong, amphid is covered with cuticle bearing minute perforations. The actual amphidial aperture, revealed only by TEM, is minute and slit-like. The apical oral aperture is reduced to a simple pore and the vestigial pharynx is devoid of an internal lumen and musculature. The mid-gut is a trophosome consisting of a solid mass of irregularly-shaped cells filled with rod-shaped structures that are assumed to be intracellular symbiotic bacteria. There is no evidence of even a vestige of a reproductive system except for the presence of the single spiculum. The phylogenetic relationships of Rhaptothyreus remain unknown. C1 Russian Fed Inst Fisheries & Oceanog, Moscow 107140, Russia. Moscow MV Lomonosov State Univ, Dept Invertebrate Zool, Moscow 125362, Russia. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Miljutin, DM (reprint author), Russian Fed Inst Fisheries & Oceanog, Verhnyaya Krasnoselskaya,17, Moscow 107140, Russia. EM dmilutin@list.ru RI Miljutin, Dmitry/A-9295-2015 OI Miljutin, Dmitry/0000-0002-0467-3021 NR 13 TC 4 Z9 5 U1 0 U2 4 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1388-5545 J9 NEMATOLOGY JI Nematology PY 2006 VL 8 BP 1 EP 20 DI 10.1163/156854106776179971 PN 1 PG 20 WC Zoology SC Zoology GA 039OI UT WOS:000237315700001 ER PT J AU Smythe, AB Nadler, SA AF Smythe, Ashleigh B. Nadler, Steven A. TI Molecular phylogeny of Acrobeloides and Cephalobus (Nematoda : Cephalobidae) reveals paraphyletic taxa and recurrent evolution of simple labial morphology SO NEMATOLOGY LA English DT Article DE 28S rRNA; free-living nematodes; morphology; probolae; sequence analysis; taxonomy ID N. SP NEMATODA; TAXONOMIC CHARACTERS; SPECIES NEMATODA; RIBOSOMAL DNA; NOTHACROBELES; REDESCRIPTION; VARIABILITY; CALIFORNIA; FRAMEWORK; STEINER AB Members of the family Cephalobidae (Nematoda) are among the most common and morphologically striking soil nematodes. Many members of Cephalobidae have extensive lip elaborations called probolae, but two taxonomically problematic genera, Acrobeloides and Cephalobus, have simple, low probolae. We sequenced a portion of the nuclear large subunit ribosomal DNA for 33 cultures of Acrobeloides and Cephalobus. A phylogenetic analysis of these data, plus sequences representing other members of Cephalobina, revealed a core clade of 22 closely related taxa, but did not represent Acrobeloides and Cephalobus as monophyletic. The dominant feature used in morphological taxonomy of Cephalobidae, the lip region, was homoplastic according to the molecular phylogenetic hypothesis. Contrary to previous suggestions, taxa with simple probolae have arisen multiple times from taxa with complex probolae. Cultures were also examined for mode of reproduction (presumed parthenogenetic vs sexual) and three morphological characters commonly used in generic diagnoses: the shape of the corpus in profile; the number of lateral incisures; and the terminal extent of the lateral field. Most cultures, including all 22 members of the core clade, lacked males and were presumed to be parthenogenetic, but several independent origins of sexually reproducing taxa were found. Of the morphological characters, only the corpus shape was consistent with the molecular phylogeny, however, the utility of this character is also questioned. Many genera with complex probolae were also paraphyletic, including Nothacrobeles, Zeldia and Cervidellus, indicating the need for more comprehensive phylogenies and a broad taxonomic revision of the family. C1 Univ Calif Davis, Dept Nematol, Davis, CA 95616 USA. RP Smythe, AB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, W-209,MRC 163,POB 37012, Washington, DC 20013 USA. EM smythea@si.edu NR 34 TC 11 Z9 15 U1 1 U2 6 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1388-5545 J9 NEMATOLOGY JI Nematology PY 2006 VL 8 BP 819 EP 836 DI 10.1163/156854106779799178 PN 6 PG 18 WC Zoology SC Zoology GA 137ND UT WOS:000244298400002 ER PT B AU Luhr, JF Kimberly, P Siebert, L Aranda-Gomez, JJ Housh, TB Mattietti, GK AF Luhr, James F. Kimberly, Paul Siebert, Lee Aranda-Gomez, J. Jorge Housh, Todd B. Mattietti, Giuseppina Kysar BE Siebe, C Macias, JL AguirreDiaz, GJ TI Mexico's Quaternary volcanic rocks: Insights from the MEXPET petrological and geochemical database SO Neogene-Quarternary Continental Margin Volcanism: A Perspective from Mexico SE GEOLOGICAL SOCIETY OF AMERICA SPECIAL PAPERS LA English DT Proceedings Paper CT Penrose Conference Neogene-Quaternary Continental Margin Volcanism - A Perspective from Mexico CY JAN 12-16, 2004 CL Puebla, MEXICO ID MIDDLE AMERICA TRENCH; EL-CHICHON VOLCANO; EAST PACIFIC RISE; SAN-LUIS-POTOSI; CALC-ALKALINE MAGMAS; SIERRA-LA-PRIMAVERA; DISEQUILIBRIUM PHENOCRYST ASSEMBLAGES; CONTINENTAL-MARGIN TRUNCATION; LOWER CRUSTAL XENOLITHS; CENOZOIC ARC VOLCANISM AB We assembled a petrological and geochemical database for Mexico's Quaternary volcanic rocks as one component of an interactive CD-ROM titled Volcanoes of Mexico. That original database was augmented to a total of 2180 records for whole-rock analyses published through May 2004 in peer-reviewed literature, supplemented by a few Ph.D. dissertations for otherwise uncovered areas. The Quaternary volcanic rocks of Mexico can be divided geographically into three tectonic settings: the Northern Mexican Extensional Province, Pacific islands, and the Mexican Volcanic Belt. The rocks also largely fall into three magma series: (1) intraplate-type alkaline, (2) calc-alkaline, and (3) lamprophyre. Many transitional varieties also exist, but we have established compositional rules to classify all samples into these three series. Intraplate-type alkaline rocks account for 30.8% of the database. Mafic intraplate-type rocks are particularly abundant at Northern Mexican Extensional Province and Pacific island volcanoes. They are characterized by strong enrichments in Ti-Ta-Nb, and many have nepheline in their CIPW norms (named for the four petrologists, Cross, Iddings, Pirsson and Washington, who devised it in 1931) and carry xenoliths of deep-crustal granulite and upper-mantle spinel and/or plagioclase peridotite. Available data indicate that significant compositional differences exist between intraplate-type mafic rocks from these two tectonic environments, with the Pacific island examples relatively depleted in Cs, Rb, Th, U, K, Ph, and Sr compared to Northern Mexican Extensional Province equivalents. Mafic intraplate-type rocks from the Camargo and San Quintin fields in the northern part of the Northern Mexican Extensional Province are relatively enriched in Pb-206/Pb-204 (19.1-19.6), indicating likely involvement of HIMU (high la) mantle in their genesis. Differentiated intraplate-type rocks (trachytes) are common at the Pacific island volcanoes, but nearly absent at the Northern Mexican Extensional Province volcanoes. Intraplate-type mafic alkaline rocks are also found in many different parts of the Mexican Volcanic Belt; we believe that the latter occurrences reflect involvement of Northern Mexican Extensional Province-type mantle sources in magma generation beneath the Mexican Volcanic Belt, where subduction-modified mantle is the dominant source feeding calc-alkaline and minor lamprophyric magmas to the surface. The calc-alkaline series, which accounts for 62.5% of the database, ranges from basalts (and lesser trachybasalts) to rhyolites but is dominated by andesites. These rocks are most prevalent in the E-W-trending, subduction-related Mexican Volcanic Belt, but are also found in Baja California, part of the Northern Mexican Extensional Province. They are characterized by enrichments in K-Ba-Sr and depletions in Ti-Ta-Nb, the classic global-scale features of subduction-related rocks. About 8.3% of the rocks from the Mexican Volcanic Belt have corundum in their CIPW norms, evidence of a significant role for sediment involvement in their petrogenesis, through either subduction of seafloor clays or contamination by pelitic lithologies during ascent through the crust. Sr and Nd isotopic data for calc-alkaline rocks from the Mexican Volcanic Belt form an array that is shifted toward higher Sr-87/Sr-86 compared to the intraplate-type suites, consistent with incorporation of subducted marine Sr. Calc-alkaline and lamprophyric rocks from Colima volcano and nearby Cantaro mark the depleted end of the Mexican Volcanic Belt isotopic array (lowest Sr-87/Sr-86 and Pb-206/Pb-204, highest epsilon(Nd)); the enriched end is marked by various basaltic andesites to rhyolites from the east-central part of the Mexican Volcanic Belt, where Mexico's continental crust reaches its maximum thickness of 40-50 km, a fact that favors crustal contamination during magma ascent. Lamprophyres account for only 6.7% of the database. True lamprophyres, with phlogopite or amphibole phenocrysts in the absence of feldspar phenocrysts, are found exclusively in the western part of the Mexican Volcanic Belt, but compositionally (not mineralogically) similar rocks are found in four volcanic fields in northern Baja California, where they have been termed bajaites, and likened to adakites. Lamprophyres have extreme subduction-related geochemical signatures, with strong enrichments in K-Ba-Sr, and equally strong relative depletions in Ti-Ta-Nb. We consider western Mexican lamprophyres to represent the "essence of subduction," partial melts of phlogopite- and apatite-rich veinlets in the subarc mantle, which are usually diluted by partial melts of the surrounding depleted peridotitic wall rocks to produce "normal" calc-alkaline magmas. Lamprophyres reached the surface in the western Mexican Volcanic Belt relatively undiluted by wall-rock melts only because of the strong extension imposed on the region by the influence of nearby plate-boundary activity. C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretoro 76001, Mexico. Inst Potosino Invest Cientif Technol, San Luis Potosi 78216, Mexico. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. George Mason Univ, Fairfax, VA 22030 USA. RP Luhr, JF (reprint author), Smithsonian Inst, Dept Mineral Sci, PO Box 37012, Washington, DC 20013 USA. NR 248 TC 11 Z9 11 U1 1 U2 5 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA BN 978-0-8137-2402-7 J9 GEOL S AM S PY 2006 IS 402 BP 1 EP 44 DI 10.1130/2006.2402(01) PG 44 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BFZ99 UT WOS:000245727600001 ER PT B AU Fenner, Y AF Fenner, Yeshe BE Kannappan, SJ Redfield, S KesslerSilacci, JE Landriau, M Drory, N TI Galactic chemical evolution SO New Horizons in Astronomy: Frank N. Bash Symposium 2005 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Frank N Bash Symposium on New Horizons Astronomy CY OCT 16-18, 2005 CL Univ Texas, Austin, TX HO Univ Texas ID GIANT BRANCH STARS; POOR HALO STARS; DWARF GALAXIES; INTERSTELLAR-MEDIUM; MILKY-WAY; METALLICITY DISTRIBUTION; ELEMENTAL ABUNDANCES; ISOTOPIC ABUNDANCES; SOLAR NEIGHBORHOOD; MG ABUNDANCES AB Stars and gas in galaxies exhibit diverse chemical element abundance patterns that are shaped by their environment and formation histories. Many generations of stars forming, synthesizing new elements, and releasing their nuclear debris when they evolve and die, are largely responsible for the abundance of the elements throughout the cosmos. By investigating Galactic Chemical Evolution (GCE), one hopes to trace the distribution of the elements from the present-day back to the early universe and in doing so, gain insight into the lives of galaxies. This review approaches the field of GCE from a theoretical perspective, describing the design, results and future prospects for models tracing the production and distribution of the elements within galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fenner, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-220-2 J9 ASTR SOC P PY 2006 VL 352 BP 145 EP 159 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFC00 UT WOS:000240947600011 ER PT J AU Lovelock, CE Feller, IC Ball, MC Engelbrecht, BMJ Ewe, ML AF Lovelock, Catherine E. Feller, Ilka C. Ball, Marilyn C. Engelbrecht, Bettina M. J. Ewe, Mei Ling TI Differences in plant function in phosphorus- and nitrogen-limited mangrove ecosystems SO NEW PHYTOLOGIST LA English DT Article DE Avicennia germinans; Belize; fertilization; Florida; hydraulic conductivity; leaf water potential; photosynthesis ID CARBON-ISOTOPE DISCRIMINATION; ROOT HYDRAULIC CONDUCTANCE; WATER-USE EFFICIENCY; RHIZOPHORA-MANGLE; NUTRIENT ENRICHMENT; GAS-EXCHANGE; FOREST TREES; PHOTOSYNTHESIS; GROWTH; LIMITATION AB Mangrove ecosystems can be either nitrogen (N) or phosphorus (P) limited and are therefore vulnerable to nutrient pollution. Nutrient enrichment with either N or P may have differing effects on ecosystems because of underlying differences in plant physiological responses to these nutrients in either N- or P-limited settings. Using a common mangrove species, Avicennia germinans, in sites where growth was either N or P limited, we investigated differing physiological responses to N and P limitation and fertilization. We tested the hypothesis that water uptake and transport, and hydraulic architecture, were the main processes limiting productivity at the P-limited site, but that this was not the case at the N-limited site. We found that plants at the P-deficient site had lower leaf water potential, stomatal conductance and photosynthetic carbon-assimilation rates, and less conductive xylem, than those at the N-limited site. These differences were greatly reduced with P fertilization at the P-limited site. By contrast, fertilization with N at the N-limited site had little effect on either photosynthetic or hydraulic traits. We conclude that growth in N- and P-limited sites differentially affect the hydraulic pathways of mangroves. Plants experiencing P limitation appear to be water deficient and undergo more pronounced changes in structure and function with relief of nutrient deficiency than those in N-limited ecosystems. C1 Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Australian Natl Univ, Res Sch Biol Sci, Canberra, ACT 0200, Australia. Smithsonian Trop Res Inst, Balboa, Panama. Tech Univ Kaiserslautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA. RP Lovelock, CE (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM c.lovelock@uq.edu.au RI 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 40 TC 40 Z9 49 U1 5 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PY 2006 VL 172 IS 3 BP 514 EP 522 DI 10.1111/j.1469-8137.2006.01851.x PG 9 WC Plant Sciences SC Plant Sciences GA 094KR UT WOS:000241238800014 PM 17083681 ER PT J AU Yahr, R Vilgalys, R DePriest, PT AF Yahr, Rebecca Vilgalys, Rytas DePriest, Paula T. TI Geographic variation in algal partners of Cladonia subtenuis (Cladoniaceae) highlights the dynamic nature of a lichen symbiosis SO NEW PHYTOLOGIST LA English DT Article DE symbiotic association; environmental specialization; Cladonia subtenuis (Cladoniaceae); lichenized fungus; specificity; selectivity ID NOSTOC-CONTAINING LICHENS; GENUS CLADONIA; DNA-SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; MONOTROPOIDEAE ERICACEAE; DETECTING RECOMBINATION; GENETIC DIVERSITY; FUNGAL ENDOPHYTES; SPECIFICITY; SYMBIODINIUM AB Multiple interacting factors may explain variation present in symbiotic associations, including fungal specificity, algal availability, mode of transmission and fungal selectivity. To separate these factors, we sampled the lichenized Cladonia subtenuis and associated Asterochloris algae across a broad geographic range. We sampled 87 thalli across 11 sites using sequence data to test for fungal specificity (phylogenetic range of association) and selectivity (frequency of association), fungal reproductive mode, and geographic structure among populations. Permutation tests were used to examine symbiont transmission. Four associated algal clades were found. Analysis of molecular variation (AMOVA) and partial Mantel tests suggested that the frequency of associated algal genotypes was significantly different among sites and habitats, but at random with respect to fungal genotype and clade. The apparent specificity for Clade II algae in the fungal species as a whole did not scale down to further within-species lineage-dependent specificity for particular algae. Fungal genotypes were not structured according to site and appeared to be recombining. We suggest that ecological specialization exists for a specific lichen partnership and a site, and that this selectivity is dynamic and environment-dependent. We present a working model combining algal availability, fungal specificity and selectivity, which maintains variation in symbiotic composition across landscapes. C1 Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. Duke Univ, Dept Biol, Durham, NC 27708 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Yahr, R (reprint author), Royal Bot Garden Edinburgh, 20A Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland. EM r.yahr@rbge.nc.uk RI DePriest, Paula/K-6633-2015; OI Vilgalys, Rytas/0000-0001-8299-3605 NR 90 TC 90 Z9 92 U1 2 U2 21 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0028-646X J9 NEW PHYTOL JI New Phytol. PY 2006 VL 171 IS 4 BP 847 EP 860 DI 10.1111/j.1469-8137.2006.01792.x PG 14 WC Plant Sciences SC Plant Sciences GA 070JJ UT WOS:000239517600016 PM 16918555 ER PT S AU Lucey, P Korotev, RL Gillis, JJ Taylor, LA Lawrence, D Campbell, BA Elphic, R Feldman, B Hood, LL Hunten, D Mendillo, M Noble, S Papike, JJ Reedy, RC Lawson, S Prettyman, T Gasnault, O Maurice, S AF Lucey, Paul Korotev, Randy L. Gillis, Jeffrey J. Taylor, Larry A. Lawrence, David Campbell, Bruce A. Elphic, Rick Feldman, Bill Hood, Lon L. Hunten, Donald Mendillo, Michael Noble, Sarah Papike, James J. Reedy, Robert C. Lawson, Stefanie Prettyman, Tom Gasnault, Olivier Maurice, Sylvestre BE Jolliff, BL Wieczorek, MA TI Understanding the lunar surface and space-moon interactions SO NEW VIEWS OF THE MOON SE Reviews in Mineralogy & Geochemistry LA English DT Review ID IMPACT-MELT BRECCIAS; ALEXANDRA RANGE 93069; LEONID METEOR-SHOWER; APOLLO 16 REGOLITH; DIGITAL-IMAGING PETROGRAPHY; NEAR-INFRARED SPECTROSCOPY; PROCELLARUM KREEP TERRANE; HEAVENLY DETECTIVE STORY; POLAR HYDROGEN DEPOSITS; ROCK-FORMING SILICATES C1 Univ Hawaii Manoa, Honolulu, HI 96822 USA. Washington Univ, St Louis, MO USA. Univ Tennessee, Knoxville, TN USA. Los Alamos Natl Lab, Los Alamos, NM USA. Smithsonian Inst, Washington, DC 20560 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Arizona, Tucson, AZ USA. Boston Univ, Cambridge, MA USA. Brown Univ, Providence, RI 02912 USA. Univ New Mexico, Albuquerque, NM 87131 USA. Northrop Grumman, Van Nuys, CA USA. Ctr Etud Spatiale Rayonnements, Toulouse, France. RP Lucey, P (reprint author), Univ Hawaii Manoa, Honolulu, HI 96822 USA. EM lucey@higp.hawaii.edu; korotev@wustl.edu RI Gasnault, Olivier/F-4327-2010; Noble, Sarah/D-7614-2012; Mendillo, Michael /H-4397-2014; OI Gasnault, Olivier/0000-0002-6979-9012; Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831 NR 549 TC 129 Z9 133 U1 4 U2 19 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1529-6466 BN 0-939950-72-3 J9 REV MINERAL GEOCHEM PY 2006 VL 60 BP 83 EP + DI 10.2138/rmg.2006.60.2 PG 144 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA BEY45 UT WOS:000240126800003 ER PT S AU Taylor, SR Pieters, CM MacPherson, GJ AF Taylor, S. Ross Pieters, Carle M. MacPherson, Glenn J. BE Jolliff, BL Wieczorek, MA TI Earth-moon system, planetary science, and lessons learned SO NEW VIEWS OF THE MOON SE Reviews in Mineralogy & Geochemistry LA English DT Review ID POLE-AITKEN BASIN; PROCELLARUM KREEP TERRANE; LUNAR SOUTH-POLE; GIANT IMPACT; RB-SR; BASALTIC VOLCANISM; OPTICAL-PROPERTIES; TOPLESS BUSHVELDS; VOLATILE ELEMENTS; MULTIRING BASINS C1 Australian Natl Univ, Dept Geol, Canberra, ACT 0200, Australia. Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Taylor, SR (reprint author), Australian Natl Univ, Dept Geol, Canberra, ACT 0200, Australia. EM Ross.Taylor@anu.edu.au NR 204 TC 23 Z9 25 U1 2 U2 14 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1529-6466 BN 0-939950-72-3 J9 REV MINERAL GEOCHEM JI Rev. Mineral. Geochem. PY 2006 VL 60 BP 657 EP 704 DI 10.2138/rmg.2006.60.7 PG 48 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA BEY45 UT WOS:000240126800008 ER PT S AU Gattobigio, GL Michaud, F Labeyrie, G Pohl, T Kaiser, R AF Gattobigio, G. L. Michaud, F. Labeyrie, G. Pohl, T. Kaiser, R. BE Drewsen, M Uggerhoj, U Knudsen, H TI Long range interactions between neutral atoms SO NON-NEUTRAL PLASMA PHYSICS VI SE AIP Conference Proceedings LA English DT Proceedings Paper CT Workshop on Non-Neural Plasmas CY JUN 25-29, 2006 CL Univ Aarhus, Aarhus, DENMARK SP QUANTOP, Danish Agcy Sci, Technol & Innovat, Carlsberg Fdn, Toyota Fdn, Danfysik HO Univ Aarhus DE long range interaction; laser cooling; instabilities ID BOSE-EINSTEIN CONDENSATION; TRAP; GAS; RADIATION; VAPOR AB In a magneto-otpical trap (MOT) where atoms can be cooled and trapped using quasi-resonant laser light, the effect of rescattered light limits the spatial density of the atoms. Here we draw an analogy between the forces associated to this multiple scattering and a Coulomb type long range interaction. A MOT in the density limited regime can thus be interpreted as a non neutral plasma with weakly charged particles. For very large samples, non linear terms in the cooling and trapping forces can lead to self sustained instabilities via a supercritical Hopf bifurcation. C1 [Gattobigio, G. L.; Michaud, F.; Labeyrie, G.; Kaiser, R.] CNRS, UMR 6618, INLN, 1361 Route Lucioles, F-06560 Valbonne, France. [Gattobigio, G. L.] Univ Ferrara, INFN, Dipartmento Fis, I-44100 Ferrara, Italy. [Pohl, T.] ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gattobigio, GL (reprint author), CNRS, UMR 6618, INLN, 1361 Route Lucioles, F-06560 Valbonne, France. RI kaiser, robin/J-3641-2014 OI kaiser, robin/0000-0001-5194-3680 FU Qudedis/ESF porgram FX T.P. acknowledges support from the Qudedis/ESF porgram NR 17 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0360-0 J9 AIP CONF PROC PY 2006 VL 862 BP 211 EP 220 PG 10 WC Physics, Fluids & Plasmas; Physics, Multidisciplinary SC Physics GA BFM64 UT WOS:000243101600026 ER PT J AU Stanley, JD Jorstad, TF Goddio, F AF Stanley, Jean-Daniel Jorstad, Thomas F. Goddio, Franck TI Human impact on sediment mass movement and submergence of ancient sites in the two harbours of Alexandria, Egypt SO NORWEGIAN JOURNAL OF GEOLOGY LA English DT Article; Proceedings Paper CT 2nd International Symposium on Submarine Mass Novements and Their Consequences CY SEP 05-07, 2005 CL Oslo, NORWAY ID LATE QUATERNARY EVOLUTION; NILE DELTA; CAESAREA MARITIMA; PATTERNS; REGION; ISRAEL AB Historic records indicate that structures built in and around the two harbours of Alexandria, Egypt, were periodically damaged by powerful events such as earthquakes and tsunamis. This geoarchaeological study reveals that human activity in nearshore and port settings has also triggered sediment deformation and construction failure. Analysis of radiocarbon-dated Holocene cores and submerged archaeological excavations record a significant incidence of sediment destabilization and mass movement in the ports since human occupation in the V millennium B.C. Anthropogenic substrate failure is documented from about the time of the city's founding by the Greeks in the 4(th) century B.C. to the present. Construction on unconsolidated sediment substrates was a factor of sediment destabilization, at times in conjunction with earthquakes, storm waves and tsunamis. Engineer reports on port construction during the past century, however, show substrate failure can also occur by building and other human activity, independently of high-energy natural events. Some recent failure and associated mass flows in the harbours were triggered by loading effects associated with emplacement of large structures on weak, water-saturated substrates. Slumps, debris flows and mudflows, initiated by substrate destabilization, caused lateral displacement of sediment and construction debris for tens of meters away from construction sites. Human-induced processes that triggered sediment failure in the ports from Greek to recent time are not likely to be unique to this sector, and findings here may help explain how some sites in coastal settings elsewhere were submerged. C1 Smithsonian Inst, NMNH, Geoarchaeol Program, Washington, DC 20013 USA. Inst Europeen Archeol Sous Marine, F-70005 Paris, France. RP Stanley, JD (reprint author), Smithsonian Inst, NMNH, Geoarchaeol Program, E-205, Washington, DC 20013 USA. EM stanleyd@si.edu NR 50 TC 8 Z9 8 U1 1 U2 5 PU GEOLOGICAL SOCIETY NORWAY PI TRONDHEIM PA C/O NGU, 7491 TRONDHEIM, NORWAY SN 0029-196X J9 NORW J GEOL JI Norw. J. Geol. PY 2006 VL 86 IS 3 BP 337 EP 350 PG 14 WC Geosciences, Multidisciplinary SC Geology GA 109HY UT WOS:000242300000019 ER PT J AU Dorr, LJ AF Dorr, LJ TI New combinations in Erica (Ericaceae : Ericoideae) from the high mountains of East Africa SO NOVON LA English DT Article DE East Africa; Erica; Ericaceae; Philippia AB Three taxa found in the high mountains of East Africa are transferred from Philippia Klotzsch to Erica L., resulting in the following new combinations: Erica johnstonii (Schweinfurth ex Engler) Dorr, E. trimera subsp. abyssinica (Pichi-Sermolli & Heiniger) Dorr, and E. trimera subsp. meruensis (R. Ross) Dorr. A neotype is selected for Philippia johnstonii Schweinfurth ex Engler, which is the basionym of E. johnstonii. A key to the five subspecies of E. trimera (Engler) Beentje also is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Dorr, LJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 19 TC 1 Z9 1 U1 2 U2 3 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PY 2006 VL 16 IS 1 BP 56 EP 58 DI 10.3417/1055-3177(2006)16[56:NCIEEE]2.0.CO;2 PG 3 WC Plant Sciences SC Plant Sciences GA 048IT UT WOS:000237941500008 ER PT S AU Brissenden, RJ Holmes, JD Mattison, E Schwartz, DA Shropshire, D AF Brissenden, Roger J. Holmes, Jeffrey D. Mattison, Edward Schwartz, Daniel A. Shropshire, Daniel BE Silva, DR Doxsey, RE TI The Chandra X-ray Center: a combined science and operations center - art. no. 627005 SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Chandra; X-ray astronomy; science center; mission operations; lessons learned ID MODEL AB The Chandra X-ray Observatory, which was launched in 1999, has to date completed almost seven years of successful science and mission operations. The Observatory, which is the third of NASA's Great Observatories, is the most sophisticated X-ray Observatory yet built. Chandra is designed to observe X-rays from high-energy regions of the universe, such as the remnants of exploded stars, environs near black holes, and the hot tenuous gas filling the void between the galaxies bound in clusters. The Chandra X-ray Center (CXC) is the focal point of scientific and mission operations for the Observatory, and provides support to the scientific community in its use of Chandra. We describe the CXC's organization, functions and principal processes, with emphasis on changes through different phases of the mission from pre-launch to long-term operations, and we discuss lessons we have learned in developing and operating a joint science and mission operations center. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brissenden, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP 27005 EP 27005 AR 627005 DI 10.1117/12.672118 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200007 ER PT S AU Paton, L AF Paton, Lisa BE Silva, DR Doxsey, RE TI Chandra hardware and systems: keeping things running - art. no. 627016 SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE computer; systems; architecture; clusters; security; user support; network AB System management for any organization can be a challenge, but satellite projects present their own issues. I will be presenting the network and system architecture chosen to support the scientists in the Chandra X-ray Center. My group provides the infrastructure for science data processing, mission planning, user support, and archive support and software development. Our challenge is to create a stable environment with enough flexibility to roll with the changes during the mission. I'll discuss system and network choices, web service, backups, security and systems monitoring. Also, how to build infrastructure that's flexible, how to support a large group of scientists with a relatively small staff, what challenges we faced (anticipated and unanticipated) and what lessons we learned over the past 6 years since the launch of Chandra. Finally I'll outline our plans for the future including Beowulf cluster support, an improved helpdesk system, and methods for dealing with the explosive amount of data that needs to be managed. C1 Smithsonian Astrophys Observ, Cambridge, MA 01749 USA. RP Paton, L (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 01749 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP 27016 EP 27016 AR 627016 DI 10.1117/12.671933 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200040 ER PT S AU Spitzbart, BD Wolk, SJ Isobe, T AF Spitzbart, Bradley D. Wolk, Scott J. Isobe, Takashi BE Silva, DR Doxsey, RE TI Chandra monitoring and trends analysis: status and lessons learned - art. no. 627018 SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Chandra; trending; real-time systems; automation AB The Chandra X-Ray Observatory was launched in July, 1999 and has yielded extraordinary scientific results. Behind the scenes, our Monitoring and Trends Analysis (MTA) approach has proven to be a valuable resource in providing telescope diagnostic information and analysis of scientific data to access Observatory performance. We have created and maintain real-time monitoring and long-term trending tools. This paper will update our 2002 SPIE paper on the design of the system and discuss lessons learned. C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Spitzbart, BD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA USA. OI Wolk, Scott/0000-0002-0826-9261 NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP 27018 EP 27018 AR 627018 DI 10.1117/12.672051 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200042 ER PT S AU Schuster, MT Marengo, M Patten, BM AF Schuster, Michael T. Marengo, Massimo Patten, Brian M. BE Silva, DR Doxsey, RE TI IRACproc: A software suite for processing and analyzing Spitzer/IRAC data - art. no. 627020 SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Spitzer Space Telescope; InfraRed Array Camera; PSF fitting; PSF subtraction ID SPACE-TELESCOPE AB We have developed a post-Basic Calibrated Data pipeline processing software suite called "IRACproc". This package facilitates the co-addition of dithered or mapped Spitzer/IRAC data to make them ready for further analysis with application to a wide variety of IRAC observing programs. In acting as a wrapper for the Spitzer Science Center's MOPEX software, IRACproc improves the rejection of cosmic rays and other transients in the co-added data. In addition, IRACproc performs (optional) Point Spread Function (PSF) fitting, subtraction, and masking of saturated stars. The under/critically sampled IRAC PSFs are subject to large variations in shape between successive frames as a result of sub-pixel shifts from dithering or telescope jitter. IRACproc improves cosmic ray and other transient rejection by using spatial derivative images to map the locations and structure of astronomical sources. By protecting sources with a metric that accounts for these large variations in the PSFs, our technique maintains the structure and photometric reliability of the PSF, while at the same time removing transients at the lowest level. High Dynamic Range PSFs for each IRAC band were obtained by combining an unsaturated core, derived from stars in the IRAC PSF calibration project, with the wings of a number of bright stars. These PSFs have dynamic ranges of similar to 10(7) and cover the entire IRAC field of view. PSF subtraction can drastically reduce the light from a bright star outside the saturated region. For a bright star near the array center it is possible to detect faint sources as close as similar to 15-20" that would otherwise be lost in the glare. In addition, PSF fitting has been shown to provide photometry accurate to 1-2% for over-exposed stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schuster, MT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 13 Z9 13 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP 27020 EP 27020 AR 627020 DI 10.1117/12.673134 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200067 ER PT S AU Adams-Wolk, NR Buehler, R Plucinsky, PP AF Adams-Wolk, Nancy R. Buehler, Royce Plucinsky, Paul P. BE Silva, DR Doxsey, RE TI The operational response to temporal changes in the gain of the ACIS instrument on the Chandra X-ray Observatory - art. no. 62701H SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE radiation damage; Chandra X-ray Observatory; space Instrumentation; X-Ray detectors; Charge-Coupled Devices (CCDs) ID CHARGE-TRANSFER INEFFICIENCY; CCD IMAGING SPECTROMETER AB The gain of the Advanced CCD Imaging Spectrometer (ACIS) instrument has changed over time since the Chandra X-ray Observatory launch in July 1999. The calibration and data analysis teams have addressed this issue, but it has only been recently that the operations team has examined how the commanding of the instrument could be altered to partially compensate for these changes. This paper will address the changes in the gain, the impact on science data and the changes the operations team has considered to improve the science return. We also discuss the restrictions imposed by the commanding software on our response. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Adams-Wolk, NR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP H2701 EP H2701 AR 62701H DI 10.1117/12.670910 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200050 ER PT S AU Drake, JJ Ratzlaff, P Kashyap, V Edgar, R Izem, R Jerius, D Siemiginowska, A Vikhlinin, A AF Drake, Jeremy J. Ratzlaff, Peter Kashyap, Vinay Edgar, Richard Izem, Rima Jerius, Diab Siemiginowska, Aneta Vikhlinin, Alexey BE Silva, DR Doxsey, RE TI Monte Carlo processes for including Chandra instrument response uncertainties in parameter estimation studies - art. no. 62701I SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Chandra X-ray Observatory; X-ray Optics; calibration; uncertainties; Monte Carlo Methods ID EFFECTIVE AREA; CALIBRATION AB Instrument response uncertainties are almost universally ignored in current astrophysical X-ray data analyses. Yet modern X-ray observatories, such as Chandra and XMM-Newton, frequently acquire data for which photon counting statistics are not the dominant source of error. Including allowance for performance uncertainties is, however, technically challenging in terms of both understanding and specifying the uncertainties themselves, and in employing them in data analysis. Here we describe Monte Carlo methods developed to include instrument performance uncertainties in typical model parameter estimation studies. These methods are used to estimate the limiting accuracy of Chandra for understanding typical X-ray source model parameters. The present study indicates that, for ACIS-S3 observations, the limiting accuracy is reached for similar to 10(4) counts. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 3 Z9 3 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP I2701 EP I2701 AR 62701I DI 10.1117/12.672226 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200051 ER PT S AU DePasquale, JM Plucinsky, PP Schwartz, DA AF DePasquale, J. M. Plucinsky, P. P. Schwartz, D. A. BE Silva, DR Doxsey, RE TI A historical fluence analysis of the radiation environment of the Chandra X-ray Observatory and implications for continued radiation monitoring - art. no. 62701J SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE CCDs; X-ray Astronomy; radiation environment; radiation damage; radiation belts; space missions AB Now in operation for over 6 years, the Chandra X-ray Observatory (CXO) has sampled a variety of space environments. Its highly elliptical orbit, with a 63.5 hr period, regularly takes the spacecraft through the Earth's radiation belts, the magnetosphere, the magnetosheath and into the solar wind. Additionally, the CXO has weathered several severe solar storms during its time in orbit. Given the vulnerability of Chandra's Charge Coupled Devices (CCDs) to radiation damage from low energy protons, proper radiation management has been a prime concern of the Chandra team. A comprehensive approach utilizing scheduled radiation safing, in addition to both on-board autonomous radiation monitoring and manual intervention, has proved successful at managing further radiation damage. However, the future of autonomous radiation monitoring on-board the CXO faces a new challenge as the multi-layer insulation (MLI) on its radiation monitor, the Electron, Proton, Helium Instrument (EPHIN), continues to degrade, leading to elevated temperatures. Operating at higher temperatures, the data from some EPHIN channels can become noisy and unreliable for radiation monitoring. This paper explores the full implication of the loss of EPHIN to CXO radiation monitoring by evaluating the fluences the CXO experienced during 40 autonomous radiation safing events from 2000 through 2005 in various hypothetical scenarios which include the use of EPHIN ill limited to no capacity as a radiation monitor. We also consider the possibility of replacing EPHIN with Chandra's High Resolution Camera (HRC) for radiation monitoring. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MD USA. RP DePasquale, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MD USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP J2701 EP J2701 AR 62701J DI 10.1117/12.672233 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200052 ER PT S AU Evans, JD Cresitello-Dittmar, M Doe, S Evans, I Fabbiano, G Germain, G Glotfelty, K Hall, D Plummer, D Zografou, P AF Evans, Janet D. Cresitello-Dittmar, Mark Doe, Stephen Evans, Ian Fabbiano, Giuseppina Germain, Gregg Glotfelty, Kenny Hall, Diane Plummer, David Zografou, Panagoula BE Silva, DR Doxsey, RE TI The Chandra X-ray Center Data System: supporting the mission of the Chandra X-ray Observatory - art. no. 62700N SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE data systems; data systems management; software maintenance; system architecture AB The Chandra X-ray Center Data System provides end-to-end scientific software support for Chandra X-ray Observatory mission operations. The data system includes the following components: (1) observers' science proposal planning tools; (2) science mission planning tools; (3) science data processing, monitoring, and trending pipelines and tools; and (4) data archive and database management. A subset of the science data processing component is ported to multiple platforms and distributed to end-users as a portable data analysis package. Web-based user tools are also available for data archive search and retrieval. We describe the overall architecture of the data system and its component pieces, and consider the design choices and their impacts on maintainability. We discuss the many challenges involved in maintaining a large, mission-critical software system with limited resources. These challenges include managing continually changing software requirements and ensuring the integrity of the data system and resulting data products while being highly responsive to the needs of the project. We describe our use of COTS and OTS software at the subsystem and component levels, our methods for managing multiple release builds, and adapting a large code base to new hardware and software platforms. We review our experiences during the life of the mission so-far, and our approaches for keeping a small, but highly talented, development team engaged during the maintenance phase of a mission. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, JD (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP N2700 EP N2700 AR 62700N DI 10.1117/12.672660 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200022 ER PT S AU McCollough, ML Rots, AH Winkelman, SL AF McCollough, Michael L. Rots, Arnold H. Winkelman, Sherry L. BE Silva, DR Doxsey, RE TI Chandra Data Archive operations: Lessons learned - art. no. 62700O SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Chandra; data archive; space based observatory; observatory operations; data processing; data distribution; X-ray AB We present a discussion of the lessons learned from establishing and operating the Chandra Data Archive (CDA). We offer an overview of the archive, what preparations were done before launch, the transition to operations, actual operations, and some of the unexpected developments that had to be addressed in running the archive. From this experience we highlight some of the important issues that need to be addressed in the creation and running of an archive for a major project. Among these are the importance of data format standards, the integration of the archive with the rest of the mission; requirements throughout all phases of the mission; operational requirements; what to expect at launch; the user interfaces; how to anticipate new tasks; and overall importance of team management and organization. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP McCollough, ML (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-67, Cambridge, MA 02138 USA. OI Rots, Arnold/0000-0003-2377-2356 NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP O2700 EP O2700 AR 62700O DI 10.1117/12.672313 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200023 ER PT S AU Nichols, J Anderson, CS Mendygral, PJ Morgan, DL Fabbiano, G AF Nichols, J. Anderson, C. S. Mendygral, P. J. Morgan, D. L. Fabbiano, G. BE Silva, DR Doxsey, RE TI Chandra data processing: Lessons learned and challenges met - art. no. 62700P SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE data processing; data operations; processing automation AB Six years into the mission, Chandra data processing operations has reached a stage of maturity that allows nearly complete automation as well as dynamic flexibility to accommodate future changes in mission and instrument status and constraints. We present a summary of the procedural and technical solutions that have been developed since the launch of Chandra to meet unanticipated challenges in the area of data processing. Lessons learned concerning data processing are discussed, including an explanation of the source of each problem and the Chandra team's response to the problem. Potential pitfalls that might affect future projects are also included. The user interface, data quality screening, and quicklook software developed specifically to address issues identified after launch have proved valuable in meeting the goals of low-cost, efficient, and flexible mission operations for the Chandra mission and can provide insight for future mission designs. C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Nichols, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP P2700 EP P2700 AR 62700P DI 10.1117/12.671757 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200024 ER PT S AU Evans, I Cresitello-Dittmar, M Doe, S Evans, J Fabbiano, G Germain, G Glotfelty, K Plummer, D Zografou, P AF Evans, Ian Cresitello-Dittmar, Mark Doe, Stephen Evans, Janet Fabbiano, Giuseppina Germain, Gregg Glotfelty, Kenny Plummer, David Zografou, Panagoula BE Silva, DR Doxsey, RE TI The Chandra X-ray Observatory data processing system - art. no. 62701U SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE data processing; pipelines; software maintenance; system architecture AB Raw data from the Chandra X-ray Observatory are processed by a set of standard data processing pipelines to create scientifically useful data products appropriate for further analysis by end users. Fully automated pipelines read the dumped raw telemetry byte stream from the spacecraft and perform the common reductions and calibrations necessary to remove spacecraft and instrumental signatures and convert the data into physically meaningful quantities that can be further analyzed by observers. The resulting data products are subject to automated validation to ensure correct pipeline processing and verify that the spacecraft configuration and scheduling matched the observers request and any constraints. In addition, pipeline processing monitors science and engineering data for anomalous indications and trending, and triggers alerts if appropriate. Data products are ingested and stored in the Chandra Data Archive, where they are made available for downloading by users. In this paper, we describe the architecture of the data processing system, including the scientific algorithms that are applied to the data, and interfaces to other subsystems. We place particular emphasis on the impacts of design choices on system integrity and maintainability. We review areas where algorithmic improvements or changes in instrument characteristics have required significant enhancements, and the mechanisms used to effect these changes while assuring continued scientific integrity and robustness. We discuss major enhancements to the data processing system that are currently being developed to automate production of the Chandra Source Catalog. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Evans, I (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP U2701 EP U2701 AR 62701U DI 10.1117/12.672641 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200061 ER PT S AU Plummer, D Grier, J Masters, S AF Plummer, David Grier, John Masters, Sreelatha BE Silva, DR Doxsey, RE TI The Chandra automated processing system: challenges, design enhancements, and lessons learned - art. no. 62701W SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE data processing; automated processing; pipelines; system architecture AB Chandra standard data processing involves hundreds of different types of data products and pipelines. Pipelines are initiated by different types of events or notifications and may depend upon many other pipelines for input data. The Chandra automated processing system (AP) was designed to handle the various notifications and orchestrate the pipeline processing. Certain data sets may require "special" handling that deviates slightly from the standard processing thread. Also, bulk reprocessing of data often involves new processing requirements. Most recently, a new type of processing to produce source catalogs has introduced requirements not anticipated by the original AP design. Managing these complex dependencies and evolving processing requirements in an efficient, flexible, and automated fashion presents many challenges. This paper describes the most significant of these challenges, the AP design changes required to address these issues and the lessons learned along the way. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Plummer, D (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-81, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP W2701 EP W2701 AR 62701W DI 10.1117/12.672293 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200063 ER PT S AU Graessle, DE Evans, IN Glotfelty, K He, XH Evans, JD Rots, AH Fabbiano, G Brissenden, RJ AF Graessle, Dale E. Evans, Ian N. Glotfelty, Kenny He, X. Helen Evans, Janet D. Rots, Arnold H. Fabbiano, Giuseppina Brissenden, Roger J. BE Silva, DR Doxsey, RE TI The Chandra X-ray Observatory calibration database (CalDB): Building, planning, and improving - art. no. 62701X SO Observatory Operations: Strategies, Processes, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE Chandra X-ray Observatory; calibration; CaIDB; pipelines; analysis software; x-ray astronomy; x-ray missions AB The calibration database implemented for the Chandra X-ray Observatory is the most detailed and extensive CalDB of its kind to date. Built according to the NASA High Energy Astrophysics Science Archive Research Center (HEASARC) CalDB prescription, the Chandra CalDB provides indexed, selectable calibration data for detector responses, mirror effective areas, grating efficiencies, instrument geometries, default source aim points, CCD characteristics, and quantum efficiencies, among many others. The combined index comprises approximately 500 entries. A standard FTOOLS parametric interface allows users and tools to access the index. Unique dataset selection requires certain input calibration parameters such as mission, instrument, detector, UTC date and time, and certain ranged parameter values. The goals of the HEASARC CalDB design are (1) to separate software upgrades from calibration upgrades, (2) to allow multi-mission use of analysis software (for missions with a compliant CalDB) and (3) to facilitate the use of multiple software packages for the same data. While we have been able to meet the multivariate needs of Chandra with the current CalDB implementation from HEASARC, certain requirements and desirable enhancements have been identified that raise the prospect of a developmental rewrite of the CalDB system. The explicit goal is to meet Chandra's specific needs better, but such upgrades may also provide significant advantages to CalDB planning for future missions. In particular we believe we will introduce important features aiding in the development of mission-independent analysis software. We report our current plans and progress. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Graessle, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Rots, Arnold/0000-0003-2377-2356 NR 4 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6270 BP X2701 EP X2701 AR 62701X DI 10.1117/12.672876 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200064 ER PT S AU Fruscione, A McDowell, JC Allen, GE Brickhouse, NS Burke, DJ Davis, JE Durham, N Elvis, M Galle, EC Harris, DE Huenemoerder, DP Houck, JC Ishibashi, B Karovska, M Nicastro, F Noble, MS Nowak, MA Primini, FA Siemiginowska, A Smith, RK Wise, M AF Fruscione, Antonella McDowell, Jonathan C. Allen, Glenn E. Brickhouse, Nancy S. Burke, Douglas J. Davis, John E. Durham, Nick Elvis, Martin Galle, Elizabeth C. Harris, Daniel E. Huenemoerder, David P. Houck, John C. Ishibashi, Bish Karovska, Margarita Nicastro, Fabrizio Noble, Michael S. Nowak, Michael A. Primini, Frank A. Siemiginowska, Aneta Smith, Randall K. Wise, Michael BE Silva, DR Doxsey, RE TI CIAO: Chandra's data analysis system SO OBSERVATORY OPERATIONS: STRATEGIES, PROCESSES, AND SYSTEMS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Observatory Operations CY MAY 25-27, 2006 CL Orlando, FL SP SPIE DE data analysis; software; X-ray astronomy; modeling and fitting ID SHERPA AB The CIAO (Chandra Interactive Analysis of Observations) software package was first released in 1999 following the launch of the Chandra X-ray Observatory and is used by astronomers across the world to analyze Chandra data as well as data from other telescopes. From the earliest design discussions, CIAO was planned as a general-purpose scientific data analysis system optimized for X-ray astronomy, and consists mainly of command line tools (allowing easy pipelining and scripting) with a parameter-based interface layered on a flexible data manipulation I/O library. The same code is used for the standard Chandra archive pipeline, allowing users to recalibrate their data in a consistent way. We will discuss the lessons learned from the first six years of the software's evolution. Our initial approach to documentation evolved to concentrate on recipe-based "threads" which have proved very successful. A multidimensional abstract approach to data analysis has allowed new capabilities to be added while retaining existing interfaces. A key requirement for our community was interoperability with other data analysis systems, leading us to adopt standard file formats and an architecture which was as robust as possible to the input of foreign data files, as well as re-using a number of external libraries. We support users who are comfortable with coding themselves via a flexible user scripting paradigm, while the availability of tightly constrained pipeline programs are of benefit to less computationally-advanced users. As with other analysis systems, we have found that infrastructure maintenance and re-engineering is a necessary and significant ongoing effort and needs to be planned in to any long-lived astronomy software. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Fruscione, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM afruscione@cfa.harvard.edu; jcm@cfa.harvard.edu OI Burke, Douglas/0000-0003-4428-7835; Houck, John/0000-0002-6761-6796; Nicastro, Fabrizio/0000-0002-6896-1364 NR 20 TC 124 Z9 124 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6335-3 J9 PROC SPIE PY 2006 VL 6270 AR 62701V DI 10.1117/12.671760 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BFB34 UT WOS:000240717200062 ER PT J AU Lang, AB Kalko, EKV Romer, H Bockholdt, C Dechmann, DKN AF Lang, AB Kalko, EKV Romer, H Bockholdt, C Dechmann, DKN TI Activity levels of bats and katydids in relation to the lunar cycle SO OECOLOGIA LA English DT Article DE lunar phobia; moonlight; activity patterns; predator; prey ID CAROLLIA-PERSPICILLATA; ARTIBEUS-JAMAICENSIS; FORAGING BEHAVIOR; MYOTIS-LUCIFUGUS; NEOTROPICAL BATS; FRUGIVOROUS BAT; MOONLIGHT; PHYLLOSTOMIDAE; PREDATION; CHIROPTERA AB Animals are exposed to many conflicting ecological pressures, and the effect of one may often obscure that of another. A likely example of this is the so-called "lunar phobia" or reduced activity of bats during full moon. The main reason for lunar phobia was thought to be that bats adjust their activity to avoid predators. However, bats can be prey, but many are carnivorous and therefore predators themselves. Thus, they are likely to be influenced by prey availability as well as predation risk. We investigated the activity patterns of the perch-hunting Lophostoma silvicolum and one of its main types of prey, katydids, to assess the influence of the former during different phases of the lunar cycle on a gleaning insectivorous bat. To avoid sampling bias, we used sound recordings and two different capture methods for the katydids, as well as video monitoring and radio-telemetry for the bats. Both, bats and katydids were significantly more active during the dark periods associated with new moon compared to bright periods around the full moon. We conclude that foraging activity of L. silvicolum is probably influenced by prey availability to a large extent and argue that generally the causes of lunar phobia are species-specific. C1 Karl Franzens Univ Graz, Neurobiol & Anim Behav Inst Zool, A-8010 Graz, Austria. Univ Ulm, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Panama City, Panama. Univ Tubingen, D-72074 Tubingen, Germany. Univ Zurich, Inst Zool, CH-8006 Zurich, Switzerland. RP Lang, AB (reprint author), Karl Franzens Univ Graz, Neurobiol & Anim Behav Inst Zool, Univ Pl 2, A-8010 Graz, Austria. EM alexander.lang@uni-graz.at RI Dechmann, Dina/A-1827-2010 NR 53 TC 66 Z9 70 U1 6 U2 40 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JAN PY 2006 VL 146 IS 4 BP 659 EP 666 DI 10.1007/s00442-005-0131-3 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 995ZX UT WOS:000234145300018 PM 16273422 ER PT J AU Kurtz, M Brody, T AF Kurtz, Michael Brody, Tim BE Jacobs, N TI The impact loss to authors and research SO OPEN ACCESS: KEY STRATEGIC, TECHNICAL AND ECONOMIC ASPECTS SE Chandos Information Professional Series LA English DT Article; Book Chapter C1 [Kurtz, Michael] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brody, Tim] Univ Southampton, Multimedia Grp, Southampton SO9 5NH, Hants, England. RP Kurtz, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009 NR 0 TC 8 Z9 8 U1 0 U2 0 PU CHANDOS PUBL PI SAWSTON PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND BN 978-1-84334-203-8 J9 CHANDOS INF PROF SER PY 2006 BP 45 EP 54 PG 10 WC Communication; Information Science & Library Science SC Communication; Information Science & Library Science GA BUI60 UT WOS:000289462500007 ER PT J AU Dahms, HU Fornshell, JA Fornshell, BJ AF Dahms, HU Fornshell, JA Fornshell, BJ TI Key for the identification of crustacean nauplii SO ORGANISMS DIVERSITY & EVOLUTION LA English DT Article DE larval instars; nauplius; identification aid; morphology; electronic key ID SCANNING ELECTRON-MICROSCOPY; LARVAL DEVELOPMENT; LIFE-CYCLE; COPEPODA; HARPACTICOIDA; ASCOTHORACIDA; THECOSTRACA; MAXILLOPODA; CIRRIPEDIA; MORPHOLOGY AB The nauplius is the earliest free-living stage in the development of most crustaceans, except in the majority of the Malacostraca. Several character states of the nauplius larva are used as constitutive for the Crustacea as a whole. The nauplius shows the following structural characters: a median (nauplius) e ye, at least three pairs of head appendages (first and second antennae, where the second antenna bears an arthrite; mandibles), a posteriorly directed fold (the labrum) extending over the mouth, and a cephalic ( = nauplius) shield. Extant taxa such as the Cephalocarida, Branchiopoda, Ostracoda, Mystacocarida, Copepoda, Cirripedia, Ascothoracida, Rhizocephala, Facetotecta, Euphausiacea, and Penaeidea are known to develop free-living nauplii. Other Crustacea show at least some vestige of an 'egg-nauplius' during embryonic development. The diversity of nauplii belonging to major crustacean taxa is briefly described, and a key to these nauplii is provided. The key is also available in digital format, as a JAVA program capable of being modified and expanded as new information arises. The programming structure allows uses in dichotomous or multi-branching formats. (c) 2005 Gesellschaft fur Biologische Systematik. Published by Elsevier GmbH. All rights reserved. C1 Hong Kong Univ Sci & Technol, Coastal Marine Lab, Kowloon, Hong Kong, Peoples R China. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Bot, Washington, DC 20560 USA. Comp & Network Support Net, Alexandria, VA 22307 USA. RP Dahms, HU (reprint author), Hong Kong Univ Sci & Technol, Coastal Marine Lab, Kowloon, Hong Kong, Peoples R China. EM hansd@ust.hk NR 78 TC 19 Z9 19 U1 2 U2 13 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1439-6092 EI 1618-1077 J9 ORG DIVERS EVOL JI Org. Divers. Evol. PY 2006 VL 6 IS 1 BP 47 EP 56 DI 10.1016/j.ode.2005.04.002 PG 10 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 013JQ UT WOS:000235406000004 ER PT B AU Kidwell, PA AF Kidwell, Peggy Aldrich BE Byers, N Williams, G TI Margaret Eliza Maltby (1860-1944) SO OUT OF THE SHADOWS: CONTRIBUTIONS OF TWENTIETH-CENTURY WOMEN TO PHYSICS LA English DT Biographical-Item; Book Chapter C1 Smithsonian Inst, Natl Museum Amer Hist, Div Informat Technol & Soc, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Informat Technol & Soc, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-521-82197-1 PY 2006 BP 26 EP 35 PG 10 WC History & Philosophy Of Science; Physics, Multidisciplinary SC History & Philosophy of Science; Physics GA BXL63 UT WOS:000296295500004 ER PT J AU De la Parra, F Jaramillo, C AF De la Parra, Felipe Jaramillo, Carlos TI The Cretaceous-Tertiary boundary in tropical latitudes: Understanding the response of tropical vegetation to a major environmental crisis SO PALYNOLOGY LA English DT Meeting Abstract C1 Smithsonian Trop Res Inst, U0948 APO AA, Miami, FL 34002 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC STRATIGRAPHIC PALYNOLOGISTS FOUNDATION PI COLLEGE STATION PA C/O VAUGHN M BRYANT, JR, PALNOLOGY LABORATORY, TEXAS A & M UNIV, COLLEGE STATION, TX 77843-4352, UNITED STATES SN 0191-6122 J9 PALYNOLOGY JI Palynology PY 2006 VL 30 BP 214 EP 214 PG 1 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 125BB UT WOS:000243415400014 ER PT J AU Mejia, P Dilcher, D Jaramillo, C AF Mejia, Paula Dilcher, David Jaramillo, Carlos TI Early angiosperm evolution in tropical latitudes SO PALYNOLOGY LA English DT Meeting Abstract C1 Univ Florida, Florida Museum Nat Hist, Paleobot & Palynol Lab, Gainesville, FL USA. Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. CTPA, Smithsonian Trop Res Inst, U0948, APO, AA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC STRATIGRAPHIC PALYNOLOGISTS FOUNDATION PI COLLEGE STATION PA C/O VAUGHN M BRYANT, JR, PALNOLOGY LABORATORY, TEXAS A & M UNIV, COLLEGE STATION, TX 77843-4352, UNITED STATES SN 0191-6122 J9 PALYNOLOGY JI Palynology PY 2006 VL 30 BP 222 EP 222 PG 1 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA 125BB UT WOS:000243415400035 ER PT J AU Clopton, JR Arnaud, PH AF Clopton, JR Arnaud, PH TI Edward Luther Kessel (1904-1997): Dipterist, professor, editor, friend - Obituary SO PAN-PACIFIC ENTOMOLOGIST LA English DT Biographical-Item C1 Santa Rosa Jr Coll, Dept Life Sci, Santa Rosa, CA 95401 USA. Calif Acad Sci, Dept Entomol, San Francisco, CA 94103 USA. Smithsonian Inst, Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Clopton, JR (reprint author), Santa Rosa Jr Coll, Dept Life Sci, 1501 Mendocino Ave, Santa Rosa, CA 95401 USA. EM parnaud@calacademy.org NR 0 TC 0 Z9 0 U1 0 U2 0 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD JAN PY 2006 VL 82 IS 1 BP 86 EP 90 PG 5 WC Entomology SC Entomology GA 053AN UT WOS:000238275900011 ER PT J AU Niven, JE AF Niven, J. E. TI Trade-offs between information processing and energy cornsumption in the evolution of insect photoreceptors SO PERCEPTION LA English DT Meeting Abstract C1 Smithsonian Trop Res Inst, Panama City, Panama. EM nivenj@si.org RI Niven, Jeremy/A-5883-2011 NR 0 TC 0 Z9 0 U1 0 U2 0 PU PION LTD PI LONDON PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND SN 0301-0066 J9 PERCEPTION JI Perception PY 2006 VL 35 SU S BP 165 EP 165 PG 1 WC Ophthalmology; Psychology; Psychology, Experimental SC Ophthalmology; Psychology GA 127PR UT WOS:000243599300521 ER PT J AU Galvez, D Cohen-Fernandez, A AF Galvez, D Cohen-Fernandez, A TI Partial compensation in Psychotria marginata (Rubiaceae) after simulated defoliation increases photon capture and photosynthesis SO PHOTOSYNTHETICA LA English DT Article DE computer modelling; daily carbon gain; photon capture ID LIGHT INTERCEPTION; CARBON GAIN; HETEROMELES-ARBUTIFOLIA; ABUTILON-THEOPHRASTI; IPOMOPSIS-AGGREGATA; FOREST UNDERSTOREY; CROWN ARCHITECTURE; CANOPY STRUCTURE; GRAZING HISTORY; TREE SEEDLINGS AB We used Y-plant, a computer-based model of plant crown architecture analysis, to simulate effects of defoliation on daily canopy carbon gain in Psychotria marginata (Rubiaceae) plants under two contrasting irradiances. Five levels of defoliation were simulated using two different types of leaf blade damage. Compensatory increases in photon-saturated photosynthetic capacity (P-max) of 25, 50, and 100 % defoliation were also simulated. In all simulations daily photon capture and CO2 assimilation increased with defoliation. However, without a compensatory response, daily canopy carbon gain also decreased with defoliation. Under high irradiance, reduction in daily canopy carbon gain was less than what would be expected if the response was proportional to leaf area reduction. Thus, 25 and 50 % defoliation resulted in only 20 and 41 % of daily canopy carbon gain reduction, respectively. In the scenario where 25 % of the leaf area was removed, if the P-max value was increased by 25 %, the remaining leaves compensated for 94 % of the daily canopy carbon relative to an undamaged non-compensated plant. At the same defoliation level, incrementing P-max values by 50 and 100 % resulted in overcompensation. Hence, because the increment of daily photon capture and CO2 assimilation after defoliation was more a passive consequence of the reduction in leaf area than an active response, under the conditions tested photosynthetic compensation could be only possible through an active mechanism such as the increment of P-max values. C1 Univ Magna, Dept Psicol, Roo 77500, Mexico. Sylvatica SC, Roo, Mexico. Smithsonian Trop Res Inst, Balboa, Panama. RP Galvez, D (reprint author), Univ Magna, Dept Psicol, Av Bonampak 371,Sm 10 Mza 2 Cancun,Q, Roo 77500, Mexico. EM david.a.galvez@gmail.com NR 50 TC 3 Z9 3 U1 1 U2 5 PU ACAD SCI CZECH REPUBLIC, INST EXPERIMENTAL BOTANY PI PRAGUE 6 PA NA KARLOVCE 1A, PRAGUE 6 CZ-160 00, CZECH REPUBLIC SN 0300-3604 J9 PHOTOSYNTHETICA JI Photosynthetica PY 2006 VL 44 IS 1 BP 46 EP 52 DI 10.1007/s11099-005-0157-0 PG 7 WC Plant Sciences SC Plant Sciences GA 012HE UT WOS:000235328100007 ER PT J AU Faust, MA AF Faust, MA TI Creation of the subgenus Testeria Faust subgen. nov. Protoperidinium Bergh from the SW Atlantic Ocean: Protoperidinium novella sp nov and Protoperidinium concinna sp nov dinophyceae SO PHYCOLOGIA LA English DT Article DE Belize; coral reef-mailgrove pond; dinoflagellates; Dinophyceae; ecology; subgenus; Testeria SUboell nov.; Protoperidinium novella sp nov.; Protoperidinium concinna sp nov.; scanning electron microscopy; taxonomy AB Two new heterotrophic Protoperidinium species are described front oceanic waters from The Gulf Stream, SW Atlantic Ocean and Belizean Atlantic Barrier Reef Ecosystems, Caribbean Sea. Protoperidinium novella Faust sp. nov. and P. concinna Faust sp. nov. show a plate formula of 4 ', la, 7 '', 4C(3+t), 6S, 5 ''', and 2 '''', which is atypical for file genus. It is characterized by a miniscule flat closure on the extreme anterior of the pointed apical horn. Apical pore complex is absent. Apical ventral plate 1 ' disconnects from the tip of the apical horn and connects directly to the anterior sulcal plate (Sa) along a straight line of the longitudinal axis of the cell's sagittal plane. The shape and position of the intercalary plate (1a) is another distinctive feature for these species, the presence of only one 1a plate. The thecal plate features of P. novella and P. concinna justifies the establishment of the new subgenus, Testeria Faust subgen. nov. The relationship with other congeneric species and the position within the genus Protoperidinium are discussed. C1 Smithsonian Inst, Dept Bot, US Natl Herbarium, Suitland, MD 20746 USA. RP Faust, MA (reprint author), Smithsonian Inst, Dept Bot, US Natl Herbarium, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM faust.maria@nmnh.edu NR 36 TC 13 Z9 14 U1 0 U2 0 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JAN PY 2006 VL 45 IS 1 BP 1 EP 9 DI 10.2216/04-62.1 PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 000WB UT WOS:000234492000001 ER PT J AU Gea-Banacloche, J Rey, AM Pupillo, G Williams, CJ Clark, CW AF Gea-Banacloche, J Rey, AM Pupillo, G Williams, CJ Clark, CW TI Mean-field treatment of the damping of the oscillations of a one-dimensional Bose gas in an optical lattice SO PHYSICAL REVIEW A LA English DT Article ID WAVES; ATOMS AB We present a theoretical treatment of the surprisingly large damping observed recently in one-dimensional Bose-Einstein atomic condensates in optical lattices. We show that time-dependent Hartree-Fock-Bogoliubov (HFB) calculations can describe qualitatively the main features of the damping observed over a range of lattice depths. We also derive a formula of the fluctuation-dissipation type for the damping, based on a picture in which the coherent motion of the condensate atoms is disrupted as they try to flow through the random local potential created by the irregular motion of noncondensate atoms. When parameters for the characteristic strength and correlation times of the fluctuations, obtained from the HFB calculations, are substituted in the damping formula, we find very good agreement with the experimentally observed damping, as long as the lattice is shallow enough for the fraction of atoms in the Mott insulator phase to be negligible. We also include, for completeness, the results of other calculations based on the Gutzwiller ansatz, which appear to work better for the deeper lattices. C1 Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. NIST, Gaithersburg, MD 20899 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Austrian Acad Sci, IQOQI, A-6020 Innsbruck, Austria. RP Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM jgeabana@uark.edu RI Clark, Charles/A-8594-2009; Williams, Carl/B-5877-2009; Gea-Banacloche, Julio/J-7546-2013 OI Clark, Charles/0000-0001-8724-9885; Gea-Banacloche, Julio/0000-0001-9482-9060 NR 29 TC 15 Z9 15 U1 1 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JAN PY 2006 VL 73 IS 1 AR 013605 DI 10.1103/PhysRevA.73.013605 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 007ZB UT WOS:000235008900131 ER PT J AU Taichenachev, AV Yudin, VI Velichansky, VL Zibrov, AS Zibrov, SA AF Taichenachev, AV Yudin, VI Velichansky, VL Zibrov, AS Zibrov, SA TI Pure superposition states of atoms generated by a bichromatic elliptically polarized field SO PHYSICAL REVIEW A LA English DT Article ID FREQUENCY STANDARD; DARK LINE; RESONANCES; VAPOR AB We identify the specific polarizations for the two components of a bichromatic field, which produce pure superposition states of atoms with a specific magnetic quantum number m via coherent population trapping. The superposition states are composed of two Zeeman substates magnetic quantum number m of the two ground-state hyperfine levels with arbitrary angular momenta F-1 and F-2. It is established that in the general case of m not equal 0, optical fields with elliptical polarizations are needed for the preparation of such a pure state. It is shown analitically that a unique advantage of the D1 line (over the D2 line) of alkali-metal atoms is the possibility that pure m-m states may be generated even if the excited-state hyperfine levels are not spectrally resolved. C1 Novosibirsk State Univ, Novosibirsk 630090, Russia. SB RAS, Inst Laser Phys, Novosibirsk 630090, Russia. RAS, PN Lebedev Phys Inst, Moscow 117924, Russia. Harvard Univ, Sch Med, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novosibirsk State Univ, Novosibirsk 630090, Russia. RI Taichenachev, Aleksei/K-7065-2015; Velichansky, Vladimir/M-4861-2015; Zibrov, Sergei/M-6400-2015; Zibrov, Alexander/G-7419-2014 OI Taichenachev, Aleksei/0000-0003-2273-0066; NR 21 TC 17 Z9 17 U1 1 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JAN PY 2006 VL 73 IS 1 AR 013812 DI 10.1103/PhysRevA.73.013812 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 007ZB UT WOS:000235008900167 ER PT J AU Zhu, C Babb, JF Dalgarno, A AF Zhu, C Babb, JF Dalgarno, A TI Theoretical study of sodium and potassium resonance lines pressure broadened by helium atoms SO PHYSICAL REVIEW A LA English DT Article ID PRECISION LIFETIME MEASUREMENTS; GAS-LASER SPECTROSCOPY; EXPERIMENTAL POTENTIALS; TRANSMISSION SPECTRA; GIANT PLANETS; BROWN DWARFS; NAHE; ATMOSPHERES; PROFILES; STATES AB We perform fully quantum mechanical calculations in the binary approximation of the emission and absorption profiles of the sodium 3s-3p and potassium 4s-4p resonance lines under the influence of a helium perturbing gas. We use carefully constructed potential energy surfaces and transition dipole moments to compute the emission and absorption coefficients at temperatures from 158 to 3000 K. Contributions from quasibound states are included. The resulting red and blue wing profiles agree well with previous theoretical calculations and with experimental measurements. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Zhu, C (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 31 Z9 31 U1 1 U2 5 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 JAN PY 2006 VL 73 IS 1 AR 012506 DI 10.1103/PhysRevA.73.012506 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 007ZB UT WOS:000235008900080 ER PT S AU Kharchenko, V AF Kharchenko, V. BE Heerikhuisen, J Florinski, V Zank, GP Pogorelov, NV TI X-ray diagnostic of the heliospheric plasma and interstellar gas SO Physics of the Inner Heliosheath: Voyager Observations, Theory, and Future Prospects SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 5th IGPP International Astrophysics Conference CY MAR 03-09, 2006 CL Honolulu, HI SP UC Riverside IGPP, Los Alamos Space Ctr, Los Alamos IGPP, Systemwide UC-IGPP DE heliosphere; charge-exchange collisions; X-rays; planetary and cometary atmospheres ID SOLAR-WIND IONS; CHARGE-EXCHANGE; ULTRAVIOLET EMISSION; CHANDRA OBSERVATIONS; C/1999 S4; SPECTRA; DISCOVERY; NEUTRALS; COMETS AB The new method of a remote diagnostic of the interacting Solar Wind (SW) plasma and neutral heliospheric gas has been recently developed, employing the charge-exchange mechanism of Extreme Ultraviolet (EUV) and X-ray emissions. Physics of collisions between heavy solar wind ions and neutral atoms and molecules from the interstellar, planetary, and cometary gases, is briefly reviewed. The charge-exchange mechanism of X-ray and EUV emissions induced by highly charged SW ions is described in detail. Unique spectra of cascading photons produced in collisions between heavy SW ions and neutral atoms or molecules are demonstrated. Emission spectra of individual SW ions are analyzed and compared with the results of recent laboratory measurements and quantal calculations. The synthetic spectra of the charge-exchange EUV and X-ray emission are constructed for the slow and fast solar wind, interacting with cometary, planetary and interstellar gases. Results of spectral modeling are compared with observational data from ROSAT, EUVE, CHIPS, FUSE, and Chandra satellite telescopes. Contribution of the charge-exchange mechanism to the diffuse Xray background is evaluated. A remote EUV and X-ray diagnostic of the SW plasma and interstellar gas is discussed. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0355-4 J9 AIP CONF PROC PY 2006 VL 858 BP 360 EP 365 PG 6 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BFK80 UT WOS:000242532200054 ER PT J AU Krause, GH Galle, A Virgo, A Garcia, M Bucic, P Jahns, P Winter, K AF Krause, GH Galle, A Virgo, A Garcia, M Bucic, P Jahns, P Winter, K TI High-light stress does not impair biomass accumulation of sun-acclimated tropical tree seedlings (Calophyllum longifolium Willd. and Tectona grandis L.f.) SO PLANT BIOLOGY LA English DT Article DE biomass accumulation; CO(2) assimilation; midday depression; photoinhibition of photosystem II; alpha-tocopherol; xanthophyll cycle; Calophyllum longifolium Willd.; Tectona grandis L.f. ID XANTHOPHYLL-CYCLE ACTIVITY; SUBOPTIMUM LEAF TEMPERATURES; THERMAL-ENERGY DISSIPATION; GOSSYPIUM-HIRSUTUM L; PHOTOSYSTEM-II; MIDDAY DEPRESSION; PHOTOSYNTHETIC CAPACITY; PHOTOCHEMICAL EFFICIENCY; CHLOROPHYLL FLUORESCENCE; CAROTENOID COMPOSITION AB Studies with seedlings of tropical rainforest trees (Calophyllum longifolium Willd.; Tectona grandis L. f.) were designed to test whether high-light stress affects photosynthetic performance and growth. Seedlings were cultivated in pots at a field site in Central Panama (9 degrees N) and separated into two groups: (1) plants exposed to full solar radiation; (2) plants subjected to automatic neutral shading (48%) whenever visible irradiance surpassed 1000, 1200, or 1600 mu mol photons m(-2) s(-1). After 2 - 4 months, chlorophyll fluorescence (F(v)/F(m) ratio), photosynthetic net CO(2) uptake, pigment composition, alpha-tocopherol content of leaves, and plant biomass accumulation were measured. Fully sun-exposed, compared to periodically shaded plants, experienced substantial high-light stress around midday, indicated by photoinhibition of photosystem II and depressed net CO(2) uptake. Higher contents of xanthophyll cycle pigments, lutein, and alpha-tocopherol showed an enhancement of photoprotection in fully sun-exposed plants. However, in all experiments, the maximum capacity of net CO(2) uptake and plant dry mass did not differ significantly between the two treatments. Thus, in these experiments, high-light stress did not impair productivity of the seedlings studied. obviously, the continuously sun-exposed plants were capable of fully compensating for any potential costs associated with photoinhibition and repair of photosystem II, reduced CO(2) assimilation, and processes of high-light acclimation. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, Univ Str 1, D-40225 Dusseldorf, Germany. EM ghkrause@uni-duesseldorf.de NR 54 TC 15 Z9 16 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1435-8603 J9 PLANT BIOLOGY JI Plant Biol. PD JAN PY 2006 VL 8 IS 1 BP 31 EP 41 DI 10.1055/s-2005-872901 PG 11 WC Plant Sciences SC Plant Sciences GA 008YP UT WOS:000235078600004 PM 16435267 ER PT S AU Karovska, M AF Karovska, Margarita BE Knezevic, Z Cvetkovic, Z Cirkovic, MM TI UV and X-ray imaging of interacting binary systems SO Proceedings of the 14th National Conference of Astronomers of Serbia and Montenegro SE PUBLICATIONS OF THE ASTRONOMICAL OBSERVATORY OF BELGRADE--SERIES LA English DT Proceedings Paper CT 14th National Conference of Astronomers of Serbia and Montenegro CY OCT 12-15, 2005 CL Belgrade, SERBIA C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL OBSERVATORY PI BELGRADE PA VOLGINA 7, BELGRADE, YUGOSLAVIA SN 0373-3742 BN 978-86-80019-07-9 J9 PUB ASTRO OBS BELGR PY 2006 IS 80 BP 117 EP 118 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFX66 UT WOS:000245309100017 ER PT J AU Wheeler, AG Henry, TJ AF Wheeler, AG Henry, TJ TI Gampsocoris decorus (Uhler) and Metacanthus tenellus Stal (Hemiptera : Berytidae): Neotropical stilt bugs as colonists of an African grass, Urochloa mutica (Poaceae), in Florida, with a review of berytid-grass associations SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Lygaeoidea; Berytidae; Gampsocorinae; Metacanthinae; Para grass; host plants; new records; grass feeding ID JALYSUS-SPINOSUS HETEROPTERA; HOST PLANTS AB Host plants of the Neotropical stilt bugs Gampsocoris decorus (Uhler) (subfamily Gampsocorinae) and Metacanthus tenellus Stal (subfamily Metacanthinae), whose U.S. distributions are limited to Southern Texas and peninsular Florida, have been un-known or little known. In Florida, both berytids have colonized Pari grass (Urochloa mutica (Forssk.) T Q. Nguyen; Poaceae), an invasive plant native to Africa. We collected G. decorus on Pari grass in 20 Counties and M. tenellus in 17 counties. Para grass is the first host plant recorded for G. decorus and first grass documented as a host for M. tenellus. Grass-feeding habits have evolved in three berytid clades and have been demonstrated for certain gampsocorines and metacanthines; grass feeding needs to be verified for bery-tine stilt bugs. C1 Clemson Univ, Dept Entomol Soil & Plant Sci, Clemson, SC 29634 USA. USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Wheeler, AG (reprint author), Clemson Univ, Dept Entomol Soil & Plant Sci, Clemson, SC 29634 USA. EM awhlr@clemson.edu; thenry@sel.barc.usda.gov NR 26 TC 2 Z9 3 U1 0 U2 0 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 JAN PY 2006 VL 108 IS 1 BP 1 EP 8 PG 8 WC Entomology SC Entomology GA 001WA UT WOS:000234572200001 ER PT J AU Robbins, RK Duarte, M AF Robbins, RK Duarte, M TI Systematic placement of Lycaena cogina Schaus (Lepidoptera : Lycaenidae : Polyommatinae), a biogeographically disjunct New World species SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID BUTTERFLIES AB Balint and Johnson described genus Elkalyce in the Lycaenopsis Section of the Polyommatini for the South American butterfly Lycaena cogina Schaus and suggested that it is closely related to the tropical Asian Oreolyce Toxopeus. This systematic placement was based on four characters that are phylogenetically uninformative or incorrect. A medial uncus Without lateral hairy lobes, cephalad entry of the ductus ejaculatorius into the penis, and brief anastomosis of forewing veins Sc and R-1 further falsify this systematic placement. Elkalyce cogina is transferred to the Everes Section of the Polyormmatini following an unpublished hypothesis from the late John Eliot, where it is likely a close relative, perhaps a congener, of the primarily eastern Asian Tongeia Tutt. Elkalyce and Tongeia are the only genera with "false" alulae, which we characterize morphologically, on the male genitalia penis, but the position of the "false" alulae in each genus is slightly different. A lectotype is designated to preserve stability of the name Lycaena cogina Schaus, and the distribution and habitat of E. cogina are summarized. Six cases are noted in which a New World lycaenid species, or species pair, is most closely related to an Old World lineage, but E. cogina is the only endemic South American lycaenid whose closest relative is in the Old World. Whether or not Elkalyce is congeneric with Tongeia, the relict distribution of E. cogina suggests extinction in the intervening areas. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. Univ Sao Paulo, Museu Zool, Colecao Lepidoptera, BR-04263000 Sao Paulo, Brazil. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 127, Washington, DC 20013 USA. EM RobbinsR@si.edu; mduartes@usp.br RI Duarte, Marcelo/K-7633-2012 NR 35 TC 3 Z9 5 U1 0 U2 0 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 JAN PY 2006 VL 108 IS 1 BP 226 EP 236 PG 11 WC Entomology SC Entomology GA 001WA UT WOS:000234572200024 ER PT S AU Wolk, SJ Bourke, TL Spitzbart, BD Megeath, ST Winston, E AF Wolk, SJ Bourke, TL Spitzbart, BD Megeath, ST Winston, E BE Wilson, A TI Chandra observations of young open clusters SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy ID STAR; LKH-ALPHA-101; REGION; NEBULA AB We review the X-ray aspects of our ongoing Chandra/Spitzer study of regions of star formation. Here we focus on three clusters. RCW 38 - one of the most massive clusters within 2 kpc, RCW 108 - a more modest O star cluster at a little more than 1 kpc away and NGC1579 a relatively nearby cluster of low mass stars surrounding the Be star LkH alpha 101. A common thread among the fields is that they are embedded with a minimum of 3 optical magnitudes of extinction. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 NR 8 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 119 EP 120 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300037 ER PT S AU Wolk, SJ AF Wolk, SJ CA Csi Org Comm BE Wilson, A TI Star formation in the era of the three great observatories: A white paper SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy AB As part of Chandra's ongoing series, a workshop was held on 13-15 July 2005, entitled: Star Formation in the Era of Three Great Observatories (http://cxc.harvard.edu/stars05). The goal of the workshop, which was co-sponsored by the Spitzer Science Center, was to develop a "white paper" which could serve as a roadmap for the star formation from space. We sought to review topics in star-formation which are inherently multiwavelength, and define both the current state of our knowledge and the points of current controversy where new observations are most needed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 121 EP 122 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300038 ER PT S AU Karovska, M AF Karovska, M BE Wilson, A TI Resolving components of the Mira AB interacting binary system SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE X-rays; binaries : symbiotic ID HUBBLE-SPACE-TELESCOPE; ULTRAVIOLET-SPECTRA; H-2 EMISSION; X-RAYS; GIANT; STARS AB Mira AB is the the nearest symbiotic binary and the only interacting binary that has been resolved from X-ray to radio wavelengths. In this paper I describe results from multiwavelength observations of Mira AB carried over the past 20 years. These include recent Chandra observations that resolved this interacting system for the first time at X-ray wavelengths. A Chandra spectrum of Mira AB and follow-up HST and ground-based observations showed evidence for an unprecedented outburst from Mira A likely associated with magnetic flare followed by a mass ejection or jet-like activity. Chandra and HST images also detect a bridge between the components, showing that Mira B is also accreting via direct mass exchange. These results have major impact on our understanding of accretion processes in other currently unresolved "wind" interacting systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 183 EP 188 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300049 ER PT S AU Fabbiano, G AF Fabbiano, G BE Wilson, A TI Investigating galaxy evolution with Chaadra SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy ID X-RAY SOURCES; FORMATION RATE INDICATOR; NUCLEAR BLACK-HOLE; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; STAR-FORMATION; COOLING FLOWS; MASS; ANTENNAE; NGC-4038/4039 AB Chandra observations show the importance of the X-ray band for studying the evolution of galaxies. Binary X-ray sources are an easily detectable tracer of the stellar population. Chandra studies of these populations are giving us insights into the nature and formation of these binaries, and provide the basis for diagnostics of galaxy evolution. With Chandra and Newton we can explore relatively poorly known aspects of the black hole population of the universe: ultra-luminous X-ray sources, that may be connected with the 'missing' intermediate mass black holes predicted by hierarchical galaxy and black hole formation scenarios; and quiescent supermassive nuclear black holes and their surroundings, as a way of understanding the fall range of the AGN phenomenon. Finally, the X-ray band provides the only way to explore hot plasma in galaxies; recent observations' are revealing the importance of these plasmas as vehicles of both chemical enrichment and energy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 49 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 391 EP 397 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300115 ER PT S AU Baldi, A Raymond, J Fabbiano, G Zezas, A Rots, A Schweizer, F King, A Ponman, T AF Baldi, A Raymond, J Fabbiano, G Zezas, A Rots, A Schweizer, F King, A Ponman, T BE Wilson, A TI The hot ISM of the antennae observed with Chandra: Discovery of chemical enrichment SO PROCEEDINGS OF THE X-RAY UNIVERSE 2005, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE galaxies : peculiar; galaxies : individual(NGC4038/39); galaxies : interactions; X-rays : galaxies; X-rays : ISM ID YOUNG STAR-CLUSTERS; INTRACLUSTER MEDIUM ENRICHMENT; HUBBLE-SPACE-TELESCOPE; X-RAY EMISSION; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; SUPERNOVA REMNANT; NGC 4038/4039; NGC-4038/4039; ABUNDANCES AB An analysis of the properties of the hot ISM in the merging pair of galaxies known as The Antennae (NGC 4038/39), performed using the deep 411 ks Chandra ACIS-S data set is presented. These deep observations and Chandra's high angular resolution allow us to investigate the properties of the hot ISM with unprecedented spatial and spectral resolution. Through a spatially resolved spectral analysis, we find a variety of temperatures (0.3-0.7 keV), densities (3 x 10(-2)-1.5 x 10(-1) cm(-3)), and N-H (up to 2 x 10(21) cm(-2)). Metal abundances for Ne, Mg, Si, and Fe vary dramatically throughout the ISM from sub-solar values (similar to 0.2) up to similar to 20 times the solar abundance. Comparison of the abundances with the average stellar yields predicted by theoretical models of SN explosions points to Type II SNe as the main contributors of metals to the hot ISM. No evidence of correlation between radiooptical star formation indicators and the metal abundances is found. Although uncertainties in the average density cannot exclude that mixing may have played some important role, the time required to produce the observed metal masses (similar to 3 Myr) suggests that the correlations are unlikely to be destroyed by the presence of efficient mixing. More likely a significant fraction of Type II SNe ejecta may be in a cool phase, in grains, or escaping in the wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abaldi@cfa.harvard.edu; pepi@cfa.harvard.edu; azezas@cfa.harvard.edu NR 38 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SPEC PUBL PY 2006 VL 604 BP 421 EP 426 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300120 ER PT S AU Elvis, M Krongold, Y Nicastro, F Brickhouse, N Binette, L AF Elvis, M Krongold, Y Nicastro, F Brickhouse, N Binette, L BE Wilson, A TI The accretion disk scale warm absorber in NGC 4051 SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy ID ACTIVE GALACTIC NUCLEI; X-RAY; LINE REGION; GALAXIES; NGC-5548 AB The warm absorber (WA) of NGC4051 is found to respond rapidly to the changing continuum in XMM EPIC-pn data, requiring high densities in the WA gas, so restricting the WA location. The two components of the WA in NGC4051 required by RGS - the 'low' and 'high' ionization phases, are determined to lie a few light-days from the ionizing continuum source, equivalent to 2200-4400 R-g The implied mass loss rates are a few percent of the accretion rate. This suggests that AGN winds are not capable of affecting galaxy-AGN co-evolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 16 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 539 EP 543 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300146 ER PT S AU Schwartz, DA Marshall, HL Gelbord, J Perlman, ES Georganopoulos, M Birkinshaw, M Worrall, DR Lovell, JE Jauncey, DL Godfrey, L Bicknell, GV Murphy, DW Jester, S AF Schwartz, DA Marshall, HL Gelbord, J Perlman, ES Georganopoulos, M Birkinshaw, M Worrall, DR Lovell, JE Jauncey, DL Godfrey, L Bicknell, GV Murphy, DW Jester, S BE Wilson, A TI The remarkable X-ray jet in the quasar 4c 20.24 SO PROCEEDINGS OF THE X-RAY UNIVERSE 2005, VOLS 1 AND 2 SE ESA Special Publications LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE jets; quasars; X-rays; 4C 20.24; PKS 1055+201 ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EXTENDED RADIO JETS; CHANDRA DISCOVERY; EMISSION; SYNCHROTRON; COMPTON; 3C-273 AB The Chandra X-ray telescope has observed a jet in 4C 20.24 (= PKS B1055+201) for which the de-projected length is inferred to be greater than 1 Mpe. The arcsec scale X-ray and 1.46 GHz jets initially follow the direction of the VLBA jet emanating N from the 0.2 mas core, but then curve to the NNW through a total change in angle of about 45 degrees. The 22 arcsec length of the jet gives us one of the best opportunities to study independent spatial elements, in order to infer how the magnetic field and relativistic beaming factor change with distance from the core. We find a constant Doppler factor of about 6, up until the radio structure bends through two 90 degree turns. The remarkable feature of this jet is that we detect extended X-ray emission of about 14 arcsec full width, symmetric about the jet. Furthermore, a similar extended X-ray feature extends to the south, where no radio or X-ray jet is visible, terminating just before the south radio lobe. At the redshift z= 1.11 of this quasar, the extended X-ray emission has a luminosity 3E44 ergs per second, comparable to a luminous X-ray cluster. This system gives us a laboratory where we can observe both the jet, and the medium with which it is interacting. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Godfrey, Leith/B-5283-2013 NR 23 TC 0 Z9 0 U1 0 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SPEC PUBL PY 2006 VL 604 BP 579 EP 584 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300153 ER PT S AU Risaliti, G Elvis, M Fabbiano, G Baldi, A Zezas, A Bianchi, S Matt, G AF Risaliti, G Elvis, M Fabbiano, G Baldi, A Zezas, A Bianchi, S Matt, G BE Wilson, A TI Extreme X-ray variability and absorption in NGC 1365 SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE galaxies : X-rays ID NGC 1365; TRANSITIONS; GALAXIES; NUCLEUS; LINES AB We present multiple Chandra and XMM-Newton observations revealing extreme X-ray absorption properties in the Seyfert Galaxy NGC 1365. We observe changes from reflection-dominated (N-H > 10(24) cm(-2)) to transmission - dominated (NH similar to 10(23) cm(-2)) states in time scales as short as three weeks; moreover, we clearly measure column density variations in the Compton thin states of similar to 10(23) cm(-2) in time scales of similar to 20, 000 sec. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Risaliti, Guido/0000-0002-3556-977X; Bianchi, Stefano/0000-0002-4622-4240 NR 7 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 655 EP 656 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300186 ER PT S 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 BE Wilson, A TI Why are they not AGN? SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE galaxies : nuclei; X-rays : galaxies AB We have studied the X-ray luminosity of the nuclear SMBH of a sample of quiescent early-type galaxies, and the inflow rate of the hot gas, feeding the SMBH. We have also studied the additional contribution of warm gas from stellar winds. Assuming an ADAF-like radiative efficiency, we find that only a fraction similar to 1-10% of the gas is accreted onto the SMBH; the rest must be removed or used to form new stars. Self-regulated feedback from the SMBH can provide the power necessary to remove the gas. Slow outflows can remove most of the mass, while a fast jet can carry out most of the accretion power. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Soria, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Graham, Alister/0000-0002-6496-9414 NR 2 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 669 EP 670 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300193 ER PT S AU Siemiginowska, A Cheung, CC LaMassa, S Burke, D Aldcroft, TL Bechtold, J Elvis, M Worrall, DM AF Siemiginowska, A Cheung, CC LaMassa, S Burke, D Aldcroft, TL Bechtold, J Elvis, M Worrall, DM BE Wilson, A TI Agn feedback and evolution of radio sources: Discovery of an X-ray cluster associated with Z=1 quasar SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE quasars : individual (3C 186); X-rays : galaxies : clusters ID COMPACT SYMMETRICAL OBJECTS; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; STEEP-SPECTRUM; 3C QUASARS; CHANDRA; GALAXIES; Z-GREATER-THAN-0.4; EMISSION; JETS AB We report the first significant detection of an X-ray cluster associated with a powerful (L-bol similar to 10(47) erg sec(-1)) radio-loud quasar at high redshift (z=1.06). Diffuse Xray emission is detected out to similar to 120 kpc from the CSS quasar 3C 186. A strong Fe-line emission at the z(rest) = 1.06 confirms its thermal nature. We find that the CSS radio source is highly overpressured with respect to the thermal cluster medium by 2-3 orders of magnitude. This provides direct observational evidence that the radio source is not thermally confined as posited in the "frustrated" scenario for CSS sources. Instead, the radio source may be young and at an early stage of its evolution. This source provides the first detection of the AGN in outburst in the center of a cooling flow cluster. Powerful radio sources are thought to be triggered by the cooling flows. The evidence for the AGN activity and intermittent outbursts comes from the X-ray morphology of low redshift clusters, which usually do not harbour quasars. 3C 186 is a young active radio source which can supply the energy into the cluster and potentially prevent its cooling. We discuss energetics related to the quasar activity and the cluster cooling flow, and possible feedback between the evolving radio source and the cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 705 EP 709 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300204 ER PT S AU Markevitch, M AF Markevitch, M BE Wilson, A TI Chandra observation of the most interesting cluster in the universe SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE galaxies : clusters : individual (1E0657-56); plasmas; X-rays : galaxies : clusters. ID TEMPERATURE; GALAXIES AB Chandra has recently observed 1E0657-56, a hot merging system at z = 0.3 (the "bullet" cluster), for 500 ks. I present some of the findings from this dataset. The cluster exhibits a prominent bow shock with M = 3.0 +/- 0.4 (one of only two known M >> 1 shock fronts), which we use for a first test of the electron-ion equilibrium in an intergalactic plasma. The temperatures across the shock are consistent with instant shock-heating of the electrons; at 95% confidence, the equilibration timescale is much shorter than the collisional Spitzer value. Global properties of 1E0657-56 are also remarkable. Despite being extremely unrelaxed, the cluster fits well on the L-X-T relation, yet its total mass estimated from the M-T relation is more than twice the value measured from lensing. This is consistent with simulations predicting that in the middle of a merger, global temperature and X-ray luminosity may be temporarily boosted by a large factor. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Markevitch, M (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 13 TC 53 Z9 53 U1 0 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 723 EP 727 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300207 ER PT S AU Steenbrugge, KC Nicastro, F Elvis, M AF Steenbrugge, KC Nicastro, F Elvis, M BE Wilson, A TI XMM-Newton RGS and Chandra LETGS observations of the WHIM in 1ES 1028+511 SO Proceedings of the X-ray Universe 2005, Vols 1 and 2 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT Symposium on the X-ray Universe 2005 CY SEP 26-30, 2005 CL El Escorial, SPAIN SP European Space Agcy DE warm-hot intergalactic medium; blazar : 1ES 1028+511; X-ray spectroscopy ID X-RAY FOREST; OBJECTS AB We report preliminary results on the detection of the Warm-Hot Intergalactic Medium (WHIM) along the line of sight toward the blazar 1ES 1028+511 (z = 0.361). 1ES 1028+511 was observed for 150 ks with the low energy transmission grating in combination with the high resolution camera onboard Chandra. An additional 300 ks observation was obtained using the reflection grating spectrometers (RGS) onboard XMM-Newton. We report the detection of three absorption lines which can be attributed to the WHIM, and compare the results with theoretical predictions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steenbrugge, KC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 11 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-915-4 J9 ESA SP PUBL PY 2006 VL 604 BP 751 EP 752 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BED92 UT WOS:000236905300217 ER PT J AU Iriarte, J AF Iriarte, J TI Vegetation and climate change since 14,810 C-14 yr BP in southeastern Uruguay and implications for the rise of early Formative societies SO QUATERNARY RESEARCH LA English DT Article DE southeastern Uruguay; paleoecolgy; archaeology; human-environment relationships; paleovegetation; phytoliths; pollen; late quaternary; mid-Holocene; early Formative ID LATE QUATERNARY; SOUTHERN BRAZIL; PHYTOLITH ASSEMBLAGES; MULTIVARIATE-ANALYSIS; HOLOCENE TRANSITION; ARAUCARIA FOREST; SAO-FRANCISCO; NORTH PAMPA; ARGENTINA; DYNAMICS AB This article presents a combined pollen and phytolith record of a 1.70-m sediment core from the wetlands of India Muerta (33 degrees 42' S, 53 degrees 57' W) in the lowland Pampa (grasslands) of southeastern Uruguay. Six C-14 dates and the pollen and phytolith content of the samples permitted the recognition of four distinct climatic periods between 14,850 C-14 yr B.P. and the present. The Late Pleistocene period (between ca. 14,810 and ca. 10,000 C-14 yr B.P.) was characterized by drier and cooler conditions indicated by the presence of a C3-dominated grassland. These conditions prevailed until the onset of the warmer and more humid climate of the Holocene around 945 0 C-14 yr B.P. The early Holocene (between around 10,000 and 6620 C-14 yr B.P.) was characterized by the establishment of wetlands in the region as evidenced by the formation of black peat, the increase in wetland taxa, and the replacement of C3 Pooideae by C4 Panicoideae grasses. During the mid-Holocene, around 6620 C-14 yr B.P., began a period of environmental change characterized by drier climatic conditions, which resulted in the expansion of halophytic communities in the flat, low-lying areas of the wetlands of India Muerta. About 4020 C-14 yr B.P. a massive spike of Amaranthaceae/Chenopodiaceae coupled with a radical drop in wetland species indicates another major and more severe period of dryness. After ca. 4000 C-14 yr B.P., a decrease of halophytic species indicates the onset of more humid and stable climatic conditions, which characterized the late Holocene. The findings reported in this article substantially improve our knowledge of the late Glacial and Holocene climate and vegetation in the region. The data provide a detailed record of the timing and severity of mid-Holocene environmental changes in southeastern South America. Significantly, the mid-Holocene drying trend coincided with major organizational changes in settlement, subsistence, and technology of the pre-Hispanic populations in the region, which gave rise to early Formative societies. This study also represents the first combined pollen and phytolith record for southeastern South America reinforcing the utility of phytoliths as significant indicators of long-term grassland dynamics. (c) 2005 University of Washington. All rights reserved. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Unit 0948, APO, AA 34002 USA. RP Iriarte, J (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Unit 0948, APO, AA 34002 USA. EM iriartej@si.edu RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 NR 66 TC 40 Z9 40 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 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD JAN PY 2006 VL 65 IS 1 BP 20 EP 32 DI 10.1016/j.yqres.2005.05.005 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 003PF UT WOS:000234693400003 ER PT S AU Kurucz, RL AF Kurucz, R. L. BE Stee, P TI Including all the lines SO RADIATIVE TRANSFER AND APPLICATIONS TO VERY LARGE TELESCOPES SE EAS PUBLICATIONS SERIES LA English DT Proceedings Paper CT GRETA Meeting 2005 CY MAY 11-13, 2005 CL Frejus, FRANCE SP GRETA ID TERM SYSTEM; AB-INITIO; CO I; SPECTRUM; DATABASE; OZONE; TIO AB We present a progress report on including all the lines in the linelists, including all the lines in the opacities, including all the lines in the model atmosphere and spectrum synthesis calculations, producing high-resolution, high-signal-to-noise atlases that show (not quite) all the lines, so that finally we can determine the properties of stars from a few of the lines. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurucz, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rkurucz@cfa.harvard.edu NR 39 TC 12 Z9 12 U1 0 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 2-86883-901-0 J9 EAS PUBLICATIONS PY 2006 VL 18 BP 129 EP 155 DI 10.1051/eas:2006009 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI30 UT WOS:000237314900008 ER PT S AU Pyrzas, S Gansicke, BT Marsh, TR Edge, A Steeghs, D Harlaftis, E AF Pyrzas, S. Gansicke, B. T. Marsh, T. R. Edge, A. Steeghs, D. Harlaftis, E. BE Solomos, NH TI RXJ0636 - A new intermediate polar SO RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 7th International Conference of the Hellenic-Astronomical-Society CY SEP 08-11, 2006 CL Lixourion, GREECE SP Municipal Lixourion Pallis, Alexander S Onassis Fdn, Hellen Minist Tourism, Hellen Astron Soc, EUDOXOS Natl Observ Educ, Prefecture Kefallinia & Ithaki, Hellen Natl Comm Astron, Hellen Naval Acad DE accretion, accretion discs; binaries : close; novae, cataclysmic variables AB We report the identification of RXJ0636 as a new intermediate polar. The system's light curves and spectral analysis, together with a variety of its physical parameters are presented. A brief description of the observations leading to the above mentioned identification is also given. C1 [Pyrzas, S.] Aristotle Univ Thessaloniki, Dept Phys, Sect Astrophys Astron & Mech, Thessaloniki 54124, Greece. [Gansicke, B. T.; Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Edge, A.] Univ Durham, Dept Phys, Durham DH1 3LH, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harlaftis, E.] Natl Observ Athens, Inst Space Applicat & Remote Sensing, GR-11810 Athens, Greece. RP Pyrzas, S (reprint author), Aristotle Univ Thessaloniki, Dept Phys, Sect Astrophys Astron & Mech, Thessaloniki 54124, Greece. RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009 OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746 NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0343-0 J9 AIP CONF PROC PY 2006 VL 848 BP 432 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFE04 UT WOS:000241381900058 ER PT S AU Tzanavaris, P Georgantopoulos, I Georgakakis, A Akylas, A Zezas, A Koulouridis, E Plionis, M AF Tzanavaris, P. Georgantopoulos, I. Georgakakis, A. Akylas, A. Zezas, A. Koulouridis, E. Plionis, M. BE Solomos, NH TI Exploring distant galaxies with Chandra SO RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 7th International Conference of the Hellenic-Astronomical-Society CY SEP 08-11, 2006 CL Lixourion, GREECE SP Municipal Lixourion Pallis, Alexander S Onassis Fdn, Hellen Minist Tourism, Hellen Astron Soc, EUDOXOS Natl Observ Educ, Prefecture Kefallinia & Ithaki, Hellen Natl Comm Astron, Hellen Naval Acad DE X-rays : galaxies; X-rays : surveys; galaxies : starburst; galaxies : active ID HAYSTACK SURVEY; CATALOG; CLASSIFICATION; NEEDLES AB We cross-correlate Chandra sources from the XAssist catalogue with the SDSS and identify galaxies which are dominated by stellar processes ('normal' galaxies). We obtain a further sample of such galaxies by also cross-correlating sources from the XBootes survey with the SDSS. We calculate photometric redshifts for this sample and combine both samples with 3 earlier samples of X-ray selected 'normal' galaxies to obtain the largest X-ray selected sample of such galaxies to date, consisting of 219 objects and spanning a range in X-ray flux fx (0.5 - 2.0 keV) approximate to 10(-13) - 10(-16) erg cm(-2) s(-1). We calculate the total sensitivity curve and number counts ('logN - logS') of 'normal' galaxies for our combined sample and compare our results with predictions from earlier work. C1 [Tzanavaris, P.; Georgantopoulos, I.; Koulouridis, E.; Plionis, M.] Natl Observ Athens, Inst Astron & Astrophys, I Metaxa & V Pavlou, Penteli 15236, Greece. [Georgakakis, A.; Akylas, A.] Imperial Coll London, Astrophys Grp, Blackett Lab, London SW7 2BZ, England. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tzanavaris, P (reprint author), Natl Observ Athens, Inst Astron & Astrophys, I Metaxa & V Pavlou, Penteli 15236, Greece. RI Georgakakis, Antonis/K-4457-2013; Koulouridis, Elias/C-4731-2014 FU Hellenic National Secretariat for Research and Technology within the framework of the Greece-USA collaboration programme Study of Galaxies with the Chandra X-ray Satellite; PPARC (UK) FX This work is funded in part by the Hellenic National Secretariat for Research and Technology within the framework of the Greece-USA collaboration programme Study of Galaxies with the Chandra X-ray Satellite. A. G. thanks PPARC (UK) for support. We acknowledge the use of data from the XMM-Newton Science Archive at VILSPA, the Chandra-XAssist archive, the High Energy Astrophysics Science Archive Research Center (HEASARC), and the NASA/IPAC Extragalactic Database (NED). NR 15 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0343-0 J9 AIP CONF PROC PY 2006 VL 848 BP 597 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFE04 UT WOS:000241381900079 ER PT B AU Rey, AM Calzetta, EA Hu, BL AF Rey, Ana M. Calzetta, Esteban A. Hu, Bei-Lok BE Hernandez, S Cataldo, H TI Bose-Einstein condensate superfluid - Mott insulator transition in an optical lattice SO Recent Progress in Many-Body Theories, Proceedings SE Series on Advances in Quantum Many-Body Theory LA English DT Proceedings Paper CT 13th International Conference on Recent Progress in Many-Body Theories CY DEC 05-09, 2005 CL Univ Buenos Aires, Buenos Aires, ARGENTINA HO Univ Buenos Aires DE Bose-Einstein condensates; phase transitions; Mott transition AB We present in this paper an analytical model for a cold bosonic gas on an optical lattice (with densities of the order of 1 particle per site) targeting the critical regime of the Bose - Einstein Condensate superfluid - Mott insulator transition. C1 Harvard Univ, Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Rey, AM (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-270-035-3 J9 SER ADV QUANT MANY B PY 2006 VL 10 BP 254 EP 257 DI 10.1142/9789812772787_0028 PG 4 WC Physics, Multidisciplinary SC Physics GA BFU91 UT WOS:000244734300028 ER PT S AU Schmieder, B Mandrini, CH Demoulin, P Pariat, E Berlicki, A DeLuca, E AF Schmieder, B. Mandrini, C. H. Demoulin, P. Pariat, E. Berlicki, A. DeLuca, E. BE Buchner, J Deng, X TI Magnetic reconfiguration before the X 17 Solar flare of October 28 2003 SO RECONNECTION AT SUN AND IN MAGNETOSPHERES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT Conference on Reconnection at Sun and in Magnetospheres held at the 35th COSPAR General Assembly CY JUL 19-20, 2004 CL Paris, FRANCE SP Comm Space Res DE sun : flare; sun : magnetic field; coronal mass ejection ID PROMINENCES AB An active region (AR) NOAA 10486, which produced a large number of X-ray flares during October-November 2003, was observed during a multi-wavelength campaign with ground based and space instruments. We focus our analysis on the observations of October 28, 2003. The magnetic field was observed with THEMIS (Na D1) and MDI (Ni I), the chromosphere with THEMIS (Ca II 8542 angstrom) and with the Meudon heliograph in H alpha, the EUV images with SOHO/EIT and TRACE. Two pre-events started just before the major X 17 flare. One was related to localized flux emergence and lasted until the decay phase of the X flare; while the second one involved a large scale quadrupolar reconnection, that we infer by modeling the AR magnetic field. Extended dimming areas across the equator (EIT), large arcades of post-flare loops (TRACE 195 angstrom) and a halo CME (LASCO) were observed consequently after the flare. We perform an extrapolation of the magnetic field above the photosphere using a linear force-free-field approximation that allows us to find the connectivity among the four polarities that would be involved in the quadrupolar reconnection event. The X 17 flare is plausibly due to the destabilisation of a twisted flux tube, the bottom part of this magnetic structure can be visualized by the presence of a filament. The destabilization is caused by converging and shearing photospheric motions towards the main magnetic inversion line. The large scale quadrupolar reconnection related to the second pre-event would favour the opening of the field above the twisted flux tube and, consequently, the coronal mass ejection. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Observ Paris, LESIA, F-92195 Meudon, France. ITA, N-0315 Oslo, Norway. UBA, IAFE, CONICET, RA-1428 Buenos Aires, DF, Argentina. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Schmieder, B (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. EM brigitte.schmieder@obspm.fr RI Buechner, Joerg/B-1213-2009; DeLuca, Edward/L-7534-2013; Berlicki, Arkadiusz/G-9001-2014 OI DeLuca, Edward/0000-0001-7416-2895; Demoulin, Pascal/0000-0001-8215-6532; NR 10 TC 16 Z9 16 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 37 IS 7 BP 1313 EP 1316 DI 10.1016/j.asr.2004.12.051 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES64 UT WOS:000239306100008 ER PT S AU Chance, K AF Chance, Kelly BE Perrin, A SariZizi, NB Demaison, J TI Spectroscopic measurements of tropospheric composition from satellite measurements in the ultraviolet and visible: Steps toward continuous pollution monitoring from space SO REMOTE SENSING OF THE ATMOSPHERE FOR ENVRIONMENTAL SECURITY SE NATO Science for Peace and Security Series C-Environmental Security LA English DT Proceedings Paper CT NATO Advanced Research Workshop on Remote Sensing of the Atmosphere for Environmental Security CY NOV 16-19, 2005 CL Rabat, MOROCCO SP NATO DE ultraviolet spectroscopy; visible spectroscopy; atmospheric remote sensing; tropospheric composition; radiative transfer modeling; chemistry and transport modeling ID ROTATIONAL RAMAN-SCATTERING; RADIATIVE-TRANSFER MODEL; CHEMICAL-TRANSPORT MODEL; RAYLEIGH-SCATTERING; ISOPRENE EMISSIONS; ATMOSPHERIC OZONE; NORTH-AMERICA; GOME; FORMALDEHYDE; RETRIEVAL AB This chapter reviews the current capabilities for ultraviolet and visible spectroscopic measurements of the Earth's troposphere, and discusses what remains to be achieved in the short term to enable global, continuous measurements of atmospheric pollution from space to be undertaken. Challenges in instrumentation, spectroscopy, radiative transfer modeling, and retrievals are discussed. Current and planned satellite instruments with the capability to make tropospheric measurements in the ultraviolet and visible, with their measurement properties, spectral coverage, and target molecules, are presented. Measurement examples are taken from recent work done at the Harvard-Smithsonian Center for Astrophysics, together with our colleagues at a number of institutions. The examples include global tropospheric ozone (O-3) measurements from the nadir geometry; global tropospheric nitrogen dioxide (NO2); bromine oxide (BrO) in the polar spring, and from salt lakes and volcanoes; global tropospheric formaldehyde (HCHO); and preliminary measurements of glyoxal (CHOCHO). Except for a few remaining developments, the field is shown to be sufficiently mature that global measurements of atmospheric pollution from space may be undertaken. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02139 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02139 USA. NR 70 TC 7 Z9 7 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1871-4668 BN 1-4020-5088-7 J9 NATO SCI PEACE SECUR JI NATO Sci. Peace Secur. Ser. C- Environ. Secur. PY 2006 BP 1 EP 25 DI 10.1007/978-1-4020-5090-9_1 PG 25 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BFO66 UT WOS:000243470300001 ER PT J AU Pukazhenthi, B Comizzoli, P Travis, AJ Wildt, DE AF Pukazhenthi, B Comizzoli, P Travis, AJ Wildt, DE TI Applications of emerging technologies to the study and conservation of threatened and endangered species SO REPRODUCTION FERTILITY AND DEVELOPMENT LA English DT Article; Proceedings Paper CT 32nd Annual Conference of the International-Embryo-Transfer-Society CY JAN 07-11, 2006 CL Orlando, FL SP Int Embryo Transfer Soc ID GERM-CELL TRANSPLANTATION; ASSISTED REPRODUCTIVE TECHNOLOGY; INTRACYTOPLASMIC SPERM INJECTION; FREEZE-DRIED SPERMATOZOA; SPERMATOGONIAL STEM-CELLS; WALLABY MACROPUS-EUGENII; WHITE-TAILED DEER; IN-VITRO; OVARIAN TISSUE; DEVELOPMENTAL COMPETENCE AB Sustaining viable populations of all wildlife species requires the maintenance of habitat, as well as an understanding of the behaviour and physiology of individual species. Despite substantial efforts, there are thousands of species threatened by extinction, often because of complex factors related to politics, social and environmental conditions and economic needs. When species become critically endangered, ex situ recovery programmes that include reproductive scientists are the usual first line of defence. Despite the potential of reproductive technologies for rapidly increasing numbers in such small populations, there are few examples of success. This is not the result of a failure on the part of the technologies per se, but rather is due to a lack of knowledge about the fundamental biology of the species in question, information essential for allowing reproductive technologies to be effective in the production of offspring. In addition, modern conservation concepts correctly emphasise the importance of maintaining heterozygosity to sustain genetic vigour, thereby limiting the practical usefulness of some procedures (such as nuclear transfer). However, because of the goal of maintaining all extant gene diversity and because, inevitably, many species are (or will become) 'critically endangered', it is necessary to explore every avenue for a potential contributory role. There are many 'emerging technologies' emanating from the study of livestock and laboratory animals. We predict that a subset of these may have application to the rescue of valuable genes from individual endangered species and eventually to the genetic management of entire populations or species. The present paper reviews the potential candidate techniques and their potential value (and limitations) to the study and conservation of rare wildlife species. C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Cornell Univ, Coll Vet Med, Baker Inst Anim Hlth, Ithaca, NY 14853 USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. RP Pukazhenthi, B (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. EM pukazhenthib@si.edu NR 146 TC 91 Z9 99 U1 2 U2 25 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1031-3613 EI 1448-5990 J9 REPROD FERT DEVELOP JI Reprod. Fertil. Dev. PY 2006 VL 18 IS 1-2 BP 77 EP 90 DI 10.1071/RD05117 PG 14 WC Developmental Biology; Reproductive Biology; Zoology SC Developmental Biology; Reproductive Biology; Zoology GA 992WA UT WOS:000233913500011 PM 16478605 ER PT J AU Thiangtum, K Swanson, WF Howard, J Tunwattana, W Tongthainan, D Wichasilpa, W Patumrattanathan, P Pinyopoommintr, T AF Thiangtum, K Swanson, WF Howard, J Tunwattana, W Tongthainan, D Wichasilpa, W Patumrattanathan, P Pinyopoommintr, T TI Assessment of basic seminal characteristics, sperm cryopreservation and heterologous in vitro fertilisation in the fishing cat (Prionailurus viverrinus) SO REPRODUCTION FERTILITY AND DEVELOPMENT LA English DT Article DE assisted reproduction; conservation; felid; genome resource banking; semen ID TIGER PANTHERA-TIGRIS; DOMESTIC CAT; FELIS-CATUS; ARTIFICIAL-INSEMINATION; ACROSOMAL INTEGRITY; FROZEN SPERMATOZOA; SEMEN; CAPACITATION; PENETRATION; CONSERVATION AB Conservation of the fishing cat, a threatened south-east Asian felid, could benefit from effective ex situ genetic management and breeding programmes, including the use of assisted reproduction. The aims of the present study were to: (1) characterise basal seminal traits of fishing cats in Thailand zoos; and (2) investigate the effect of cryopreservation on sperm motility, acrosomal integrity and in vitro function. Seminal traits were evaluated in electroejaculates collected from eight males. Spermatozoa were diluted in n-tris(hydroxymethyl)-methyl-2aminoethanesulfonic acid Tris (TEST)-yolk buffer (TYB) without glycerol, then diluted further with TYB with glycerol (4% final concentration) at either 25 degrees C or after slow cooling to 5 degrees C and frozen in straws over liquid nitrogen vapour. After thawing, sperm function was assessed by insemination of viable domestic cat oocytes. Fishing cat ejaculates averaged (+/- s.e.m.) 43.6 +/- 14.2 x 10(6) motile spermatozoa with 33.5 +/- 6.8% normal sperm morphology. Semen processing had a negligible effect (P > 0.05) on sperm motility and acrosomal integrity, but values were reduced (P < 0.05) after thawing. All thawed samples fertilised domestic cat oocytes, with 62.1% (36/58) of mature oocytes cleaving. Glycerol addition at 5 degrees C resulte in higher (P < 0.05) post-thaw motility and intact acrosomes than glycerol addition at 25 degrees C. In conclusion, good-quality ejaculates can be obtained from Thai fishing cats and their spermatozoa exhibit adequate function after cryopreservation for in vitro fertilisation procedures. C1 Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, Cincinnati, OH 45220 USA. Kasetsart Univ, Agr Biotechnol Ctr, Nakhon Pathom 73140, Thailand. Smithsonian Inst, Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. Khao Kheow Open Zoo, Chon Buri 20210, Thailand. Dusit Zoo, Bangkok 10300, Thailand. Khao Pratupchang Wildlife Breeding Ctr, Dept Natl Pk Wildlife & Plant Conservat, Rachaburi 70150, Thailand. RP Swanson, WF (reprint author), Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife, 3400 Vine St, Cincinnati, OH 45220 USA. EM william.swanson@cincinnatizoo.org FU NCRR NIH HHS [RR015388] NR 50 TC 22 Z9 22 U1 1 U2 11 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1031-3613 EI 1448-5990 J9 REPROD FERT DEVELOP JI Reprod. Fertil. Dev. PY 2006 VL 18 IS 3 BP 373 EP 382 DI 10.1071/RD05098 PG 10 WC Developmental Biology; Reproductive Biology; Zoology SC Developmental Biology; Reproductive Biology; Zoology GA 008UE UT WOS:000235065400008 PM 16554013 ER PT B AU Moran, JM AF Moran, James M. BE Backer, DC Turner, JL Moran, JM TI The submillimeter array SO Revealing the Molecular Universe: One Antenna is Never Enough: IN HONOR OF THE ACADEMIC RETIREMENT OF JACK WELCH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on Revealing the Molecular Universe - One Antenna is Never Enough CY SEP 09-10, 2005 CL Univ Berkeley, Berkeley, CA HO Univ Berkeley ID SAGITTARIUS-A-ASTERISK; LINEAR-POLARIZATION; GHZ; SIZE AB The origin, history and scientific rationale of the Submillimeter Array project, which dates back to 1983, are described. The current, capabilities of, and the planned improvements for, the instrument are also discussed. Jack Welch contributed enormously to the project as an informal advisor, and also as the chair of the Advisory Committee for thirteen years. Interesting excerpts from the Committee's reports are reviewed. Finally, some of the initial scientific results related to Jack's interests and to work at BIMA are described. These include observations of Pluto-Charon, the star forming regions NGC1333 and HH211, and Sgr A*. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moran, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-24-2 J9 ASTR SOC P PY 2006 VL 356 BP 45 EP 57 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BGA64 UT WOS:000245811400005 ER PT B AU Ho, PTP AF Ho, Paul T. P. BE Backer, DC Turner, JL Moran, JM TI Musings from a welch foot-soldier: Formation of massive stars SO Revealing the Molecular Universe: One Antenna is Never Enough: IN HONOR OF THE ACADEMIC RETIREMENT OF JACK WELCH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on Revealing the Molecular Universe - One Antenna is Never Enough CY SEP 09-10, 2005 CL Univ Berkeley, Berkeley, CA HO Univ Berkeley AB The formation of massive stars has always been one of Jack's scientific interests. For old people, this is easy to understand. It is because massive stars are bright, and easy to detect with little interferometers, which might have only one baseline. For tough guys and gals, this is also easy to understand. Low-mass stars are too simple, useful only for theoreticians to contemplate: High-mass stars will be where the important physics phenomena lie. All of Jack's friends know lie has never been, and never will be, old, and lie is tougher than he appears. C1 Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ho, PTP (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-24-2 J9 ASTR SOC P PY 2006 VL 356 BP 243 EP 250 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BGA64 UT WOS:000245811400026 ER PT B AU Chen, HR Welch, WJ Wilner, DJ Sutton, EC AF Chen, Huei-Ru Welch, William J. Wilner, David J. Sutton, Edmund C. BE Backer, DC Turner, JL Moran, JM TI A massive protobinary system in the hot core W3(H2O) SO Revealing the Molecular Universe: One Antenna is Never Enough: IN HONOR OF THE ACADEMIC RETIREMENT OF JACK WELCH SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on Revealing the Molecular Universe - One Antenna is Never Enough CY SEP 09-10, 2005 CL Univ Berkeley, Berkeley, CA HO Univ Berkeley ID H2O MASER SOURCE; W3(OH) AB We used the BIMA array to observe the hot molecular core W3(E2O). Our continuum maps at wavelengths of 1.4mm and 2.8mm both achieve sub-aresecond angular resolutions and show a double-peaked morphology. The angular separation of the two sources is 1."19 corresponding to 2.43 x 10(3) AU at the source distance of 2.04 kpc. The flux densities of the two sources at lambda lambda 1.4nnn and 2.8mm have a spectral index of 3, translating to an opacity law of kappa(v) alpha v. The small spectral indices suggest that grain growth has begun in the hot core. We have also observed 5 of the K-components of the methyl cyanide (CH3CN) J = 12-11 transition. A radial velocity difference of 2.81 km s(-1) is found for the gas in the two continuum peaks. Interpreting these two sources as binary components in orbit about one another, we find a minimum mass of 22 M-circle dot for the system. Power-law density distributions close to the free-fall value, r(-1.5), are found for both components, suggesting continuing accretion. The derived luminosities suggest the two sources have equivalent zero-age main sequence (ZAMS) spectral type 130.5 - B0. A velocity gradient previously detected. may be explained by unresolved binary rotation with a small velocity difference. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 115, 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, Taipei 115, Taiwan. NR 6 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-24-2 J9 ASTR SOC P PY 2006 VL 356 BP 270 EP 274 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BGA64 UT WOS:000245811400030 ER PT S AU McLeod, B Geary, J Ordway, M Amato, S Conroy, M Gauron, T AF McLeod, Brian Geary, John Ordway, Mark Amato, Steven Conroy, Maureen Gauron, Thomas BE Beletic, JE Beletic, JW Amico, P TI THE MMT MEGACAM - Focal plane design and performance SO SCIENTIFIC DETECTORS FOR ASTRONOMY 2005: EXPLORERS OF THE PHOTON ODYSSEY SE Astrophysics and Space Science Library LA English DT Proceedings Paper CT Workshop on Scientific Detectors for Astronomy CY JUN 19-25, 2005 CL Taormina, ITALY SP e2v technologies, GL Sci, Ist Nazl Astrofis, Raytheon Vis Syst, Rockwell Sci Co, ST Microelect, Fairchild Imaging, Hitec2000, Medianet Comunicazioni, Reg Siciliana, SciMeasure Analyt Syst, Univ Catania DE MMT Megacam; mosaic cameras AB The MMT Megacam is a mosaic camera with 36 2048x4608 pixel CCDs, covering a 25'x25'field of view and mounted at the f/5 Cassegrain focus of the 6.5 m MMT. Megacam was commissioned in November 2003 and has been conducting scientific observations since then. In this paper we describe some of the design and performance characteristics of the Megacam focal plane. C1 [McLeod, Brian; Geary, John; Ordway, Mark; Amato, Steven; Conroy, Maureen; Gauron, Thomas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McLeod, B (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM bmcleod@cfa.harvard.edu NR 3 TC 16 Z9 16 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 1-4020-4329-5 J9 ASTROPHYS SPACE SC L PY 2006 VL 336 BP 337 EP + DI 10.1007/1-4020-4330-9_37 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEK77 UT WOS:000237613100037 ER PT S AU Bemporad, A Poletto, G Raymond, JC AF Bemporad, A. Poletto, G. Raymond, J. C. BA Jorda, L BF Jorda, L BE Worms, JC Anselmo, L TI Evidence for pyroxene dust grains in C/2001 C2 sungrazing comet SO SMALL BODIES IN THE SOLAR SYSTEM; SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE comets; general; comets; individual (C/2001 C2); spectroscopy; EUV ID SOLAR; COLLISIONS; UVCS AB In this paper we analyze SOHO/UVCS data of the sungrazing comet C/2001 C2, a member of the Kreutz family, that was observed on February 7, 2001, at the heliocentric distances of 4.98 and 3.60 solar radii. This comet splits in a main nucleus and a fragment which have been identified in UV data. A study of the cometary Hydrogen Ly alpha emission from these two objects revealed that the Lya signal from the fragment decays exponentially with time, while the signal from the main object consists of an exponentially decaying term superposed onto a constant background. The latter emission has been ascribed to the sublimation of pyroxene dust grains, whose end products neutralize coronal protons via charge exchange processes. This interpretation allowed us to estimate, for the first time, the number density of pyroxene dust grains in a sungrazing comet. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bemporad, A.] Univ Florence, Dept Astron, Lgo E Fermi 2, I-50125 Florence, Italy. [Poletto, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bemporad, A (reprint author), Univ Florence, Dept Astron, Lgo E Fermi 2, I-50125 Florence, Italy. EM bemporad@arcetri.astro.it; poletto@arcetri.astro.it; jraymond@cfa.harvard.edu FU NASA [NAG5-12814]; COFIN [2003029124_003]; ESA; NASA FX The authors thank Dr. S. Cranmer and Dr. G. Tozzi for useful discussions. This work was supported by NASA grant NAG5-12814 and COFIN 2003029124_003; SOHO is a mission of international cooperation between ESA and NASA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 9 BP 1972 EP + DI 10.1016/j.asr.2005.10.005 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW07 UT WOS:000245035100012 ER PT S AU Frisch, PC Slavin, JD AF Frisch, Priscilla C. Slavin, Jonathan D. BE Frisch, PC TI SHORT-TERM VARIATIONS IN THE GALACTIC ENVIRONMENT OF THE SUN SO SOLAR JOURNEY: THE SIGNIFICANCE OF OUR GALACTIC ENVIRONMENT FOR THE HELIOSPHERE AND EARTH SE Astrophysics and Space Science Library LA English DT Article; Book Chapter DE Interstellar Matter; Heliosphere; Equilibrium Models ID LOCAL INTERSTELLAR-MEDIUM; ABSORPTION-LINE SURVEY; HIGH-RESOLUTION SURVEY; INTER-STELLAR MEDIUM; EXTREME-ULTRAVIOLET EXPLORER; MAGNETIC-FIELD; SOLAR-WIND; OF-SIGHT; CA-II; DEUTERIUM ABUNDANCE AB The galactic environment of the Sun varies over short timescales as the Sun and interstellar clouds travel through space. Small variations in the dynamics, ionization, density, and magnetic field strength in the interstellar medium (ISM) surrounding the Sun can lead to pronounced changes in the properties of the heliosphere. The ISM within similar to 30 pc consists of a group of cloudlets that flow through the local standard of rest with a bulk velocity of similar to 17-19 km s(-1), and an upwind direction suggesting an origin associated with stellar activity in the Scorpius-Centaurus association. The Sun is situated in the leading edge of this flow, in a partially ionized warm cloud with a density of similar to 0.3 cm(-3). Radiative transfer models of this tenuous ISM show that the fractional ionization of the ISM, and therefore the boundary conditions of the heliosphere, will change from radiative transfer effects alone as the Sun traverses a tenuous interstellar cloud. Ionization equilibrium is achieved for a range of ionization levels, depending on the ISM parameters. Fractional ionization ranges of chi(H) = 0.16-0.27 and chi(He) = 0.19-0.34 are found for tenuous clouds in equilibrium. In addition, both temperature and velocity vary between clouds. Cloud densities derived from these models permit primitive estimates of the cloud morphology, and the timeline for the Sun's passage through interstellar clouds for the past and future similar to 10(5) years. The most predictable transitions happen when the Sun emerged from the near vacuum of the Local Bubble interior and entered the cluster of local interstellar clouds flowing past the Sun, which appears to have occurred sometime during the past 44,000-150,000 years, and again when the Sun entered the local interstellar cloud now surrounding and inside of the solar system, which occurred sometime within the past 45,000 years, possibly a 1000 years ago. Prior to 150,000 years ago, no interstellar neutrals would have entered the solar system, so the pickup ion and anomalous cosmic ray populations would have been absent. The tenuous ISM within 30 pc is similar to low column density material observed globally. In this chapter, we review the factors important to understanding short-term variations in the galactic environment of the Sun. Most ISM within 40 pc is partially ionized warm material, but an intriguing possibility is that tiny cold structures may be present. C1 [Frisch, Priscilla C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. EM frisch@oddjob.uchicago.edu; jslavin@cfa.harvard.edu; frisch@oddjob.uchicago.edu NR 151 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 978-1-4020-4397-0 J9 ASTROPHYS SPACE SC L PY 2006 VL 338 BP 133 EP 193 DI 10.1007/1-4020-4557-3_6 D2 10.1007/1-4020-4557-3 PG 61 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJN25 UT WOS:000266841500006 ER PT S AU Borde, PJ Traub, WA Kern, BD Trauger, JT Kuhnert, AC AF Borde, Pascal J. Traub, Wesley A. Kern, Brian D. Trauger, John T. Kuhnert, Andreas C. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Speckle nulling for exoplanet detection with space-based coronagraphic telescopes - art. no. 62651C SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE high-contrast imaging; coronagraphy; Adaptive Optics; exoplanets ID DEFORMABLE MIRROR AB To detect Earth-like planets in the visible with a coronagraphic telescope, two major noise sources have to be overcome: the photon noise of the diffracted star light, and the speckle noise due to the star light scattered by instrumental defects. Coronagraphs tackle only the photon noise contribution. In order to decrease the speckle noise below the planet level, an active control of the wave front is required. We have developed analytical methods to measure and correct the speckle noise behind a coronagraph with a deformable mirror. In this paper, we summarize these methods, present numerical simulations, and discuss preliminary experimental results obtained with the High-Contrast Imaging Testbed at NASA's Jet Propulsion Laboratory. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Borde, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP C2651 EP C2651 AR 62651C DI 10.1117/12.670553 PN 1-2 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400039 ER PT S AU Tolls, V Aziz, M Gonsalves, RA Korzennik, S Labeyrie, A Lyon, R Melnick, G Schlitz, R Somerstein, S Vasudevan, G Woodruff, R AF Tolls, Volker Aziz, Michael Gonsalves, Robert A. Korzennik, Sylvain Labeyrie, Antoine Lyon, Richard Melnick, Gary Schlitz, Ruth Somerstein, Steve Vasudevan, Gopal Woodruff, Robert BE Mather, JC MacEwen, HA DeGraauw, MWM TI Study of coronagraphic techniques - art. no. 62653K SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE AB Smithsonian Astrophysical Observatory (SAO) has set up a program to study coronagraphic techniques. The program consists of the development of new fabrication methods of occulter masks, characterization of the manufactured masks, and application of the masks to study speckle reduction technique. Our occulter mask fabrication development utilizes a focused ion beam system to directly shape mask profiles from absorber material. Initial milling trials show that we can shape nearly Gaussian-shaped mask profiles. Part of this development is the characterization of absorber materials, poly(methyl methacrylate) doped with light-stable chromophores. For the characterization of the masks we have built a mask scanner enabling us to scan the transmission function of occulter masks. The real mask transmission profile is retrieved applying the maximum entropy method to deconvolve the mask transmission function from the beam profile of the test laser. Finally, our test bed for studying coronagraphic techniques is nearing completion. The optical setup is currently configured as a classical coronagraph and can easily be re-configured for studying speckle reduction techniques. The development of the test bed control software is under way. This paper we will give an update of the status of the individual program elements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tolls, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Lyon, Richard/D-5022-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP K2653 EP K2653 AR 62653K DI 10.1117/12.672647 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400107 ER PT S AU Romaine, S Basso, S Bruni, RJ Burkert, W Citterio, O Conti, G Engelhaupt, D Freyberg, MJ Ghigo, M Gorenstein, P Gubarev, M Hartner, G Mazzoleni, F O'Dell, S Pareschi, G Ramsey, BD Speegle, C Spiga, D AF Romaine, S. Basso, S. Bruni, R. J. Burkert, W. Citterio, O. Conti, G. Engelhaupt, D. Freyberg, M. J. Ghigo, M. Gorenstein, P. Gubarev, M. Hartner, G. Mazzoleni, F. O'Dell, S. Pareschi, G. Ramsey, B. D. Speegle, C. Spiga, D. BE Turner, MJL Hasinger, G TI Development of a prototype nickel optic for the Constellation-X hard X-ray telescope: IV - art. no. 62661C SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray Telescopes; X-ray optics; multilayers; electroformed optics ID MISSION; MULTILAYERS; MIRRORS; MSFC AB The Constellation-X mission planned for launch in 2015-2020 timeframe, will feature an array of Hard X-ray telescopes (HXT) with a total collecting area greater than 1500 cm(2) at 40 keV. Two technologies are being investigated for the optics of these telescopes, one of which is multilayer-coated Electroformed-Nickel-Replicated (ENR) shells. The attraction of the ENR process is that the resulting full-shell optics are inherently stable and offer the prospect of better angular resolution which results in lower background and higher instrument sensitivity. We are building a prototype HXT mirror module using an ENR process to fabricate the individual shells.This prototype consists of 5 shells with diameters ranging from 15 cm to 28 cm with a length of 42.6 cm. The innermost of these will be coated with iridium, while the remainder will be coated with graded d-spaced W/Si multilayers. The assembly structure has been completed and last year we reported on full beam illumination results from the first test shell mounted in this structure. We have now fabricated and coated two (15 cm and 23 cm diameter) 100 micron thick shells which have been aligned and mounted. This paper presents the results of full beam illumination X-ray tests, taken at MPE-Panter. The HEW of the individual shells will be discussed, in addition to results from the full two shell optic test. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Spiga, Daniele/0000-0003-1163-7843; O'Dell, Stephen/0000-0002-1868-8056; Ghigo, Mauro/0000-0003-2284-9251; Pareschi, Giovanni/0000-0003-3967-403X NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP C2661 EP C2661 AR 62661C DI 10.1117/12.672052 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400041 ER PT S AU Elvis, M Brissenden, RJ Fabbiano, G Schwartz, DA Reid, P Podgorski, W Eisenhower, M Juda, M Phillips, J Cohen, L Wolk, S AF Elvis, Martin Brissenden, R. J. Fabbiano, G. Schwartz, D. A. Reid, P. Podgorski, W. Eisenhower, M. Juda, M. Phillips, J. Cohen, L. Wolk, S. BE Turner, MJL Hasinger, G TI Active X-ray optics for Generation-X, the next high resolution X-ray observatory - art. no. 62661K SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray optics; active optics; X-ray astronomy ID INTERGALACTIC MEDIUM; CHANDRA; PERFORMANCE; POPULATION; SPRING-8; ANTENNAE; MASS AB X-rays provide one of the few bands through which we can study the epoch of reionization, when the first galaxies, black holes and stars were born. To reach the sensitivity required to image these first discrete objects in the universe needs a major advance in X-ray optics. Generation-X (Gen-X) is currently the only X-ray astronomy mission concept that addresses this goal. Gen-X aims to improve substantially on the Chandra angular resolution and to do so with substantially larger effective area. These two goals can only be met if a mirror technology can be developed that yields high angular resolution at much lower mass/unit area than the Chandra optics, matching that of Constellation-X (Con-X). We describe an approach to this goal based on active X-ray optics that correct the mid-frequency departures from an ideal Wolter optic on-orbit. We concentrate on the problems of sensing figure errors, calculating the corrections required, and applying those corrections. The time needed to make this in-flight calibration is reasonable. A laboratory version of these optics has already been developed by others and is successfully operating at synchrotron light sources. With only a moderate investment in these optics the goals of Gen-X resolution can be realized. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Juda, Michael/0000-0002-4375-9688; Wolk, Scott/0000-0002-0826-9261 NR 24 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP K2661 EP K2661 AR 62661K DI 10.1117/12.672072 PN 1-2 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400048 ER PT S AU Elvis, M AF Elvis, Martin BE Turner, MJL Hasinger, G TI The Extreme Physics Explorer SO SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray optics; spectroscopy; polarimetry; timing; neutron stars; black holes; magnetars; fundamental physics ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; X-RAY PULSARS; BLACK-HOLE; ACCRETION DISK; GRAVITY-WAVES; POLARIZATION; EMISSION; RADIATION; SPECTRA AB Some tests of fundamental physics - the equation of state at supra-nuclear densities, the metric in strong gravity, the effect of magnetic fields above the quantum critical value - can only be measured using compact astrophysical objects: neutron stars and black holes. The Extreme Physics Explorer is a modest sized (similar to 500 kg) mission that would carry a high resolution (R similar to 300) X-ray spectrometer and a sensitive X-ray polarimeter, both with high time resolution (similar to 5 mu s) capability, at the focus of a large area (similar to 5 sq.m), low resolution (HPD similar to 1 arcmin) X-ray mirror. This instrumentation would enable new classes of tests of fundamental physics using neutron stars and black holes as cosmic laboratories. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elvis@cfa.harvard.edu NR 45 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6331-0 J9 PROC SPIE PY 2006 VL 6266 AR 62660Q DI 10.1117/12.672053 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400022 ER PT S AU Plucinsky, PP DePasquale, JM Snowden, SL AF Plucinsky, Paul P. DePasquale, Joseph M. Snowden, Steven L. BE Turner, MJL Hasinger, G TI Verifying the low-energy spectral response models of the CXO ACIS and XMM-Newton EPIC CCDs SO SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE Chandra X-ray Observatory; XMM-Newton; ACIS; EPIC; charge-coupled devices (CCDs); X-ray detectors; X-ray spectroscopy ID SUPERNOVA REMNANT 1E-0102.2-7219; PHOTON IMAGING CAMERA; X-RAY-SPECTRUM; INSTRUMENT; SPECTROMETER AB The flight calibration of the spectral response of CCD instruments below 1.5 keV is difficult in general because of the lack of strong lines in the on-board calibration sources typically used and the relatively poor spectral resolution at the lowest energies. We used 1E 0102.2-7219 (the brightest supernova remnant in the SMC) to evaluate the response models of the ACIS CCDs on the Chandra X-ray Observatory and the EPIC CCDs on the XMM-Newton Observatory. E0102 has strong lines of 0, Ne, and Mg below 1.5 keV and very little or no Fe emission to complicate the spectrum. The spectrum of E0102 has been well-characterized using the gratings on the CXO and XMM-Newton. We have used the high-resolution spectral data from both gratings instruments to develop a spectral model for the CCD spectra. Fits with this model are sensitive to any problems with the gain calibration and the spectral redistribution model. We have also used the measured intensities of the lines to investigate the consistency of the detection efficiency models for the different instruments. We find that the gain of the three instruments is accurate to within 1.1% at similar to 570 eV and 0.9% at similar to 910 eV. We find that the measured flux of the Ne X Ly alpha line agrees at the 90% confidence limit for all detectors (within 6%). We find significant differences in the measured flux of the O VIII Ly alpha line, the largest discrepancy between one pair of datasets is 18%. Further analysis is required to investigate this discrepancy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plucinsky, PP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM plucinsky@cfa.harvard.edu NR 21 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6331-0 J9 PROC SPIE PY 2006 VL 6266 AR 62662Q DI 10.1117/12.671653 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400082 ER PT S AU Walsworth, RL AF Walsworth, R. L. BE Ehlers, J Lammerzahl, C TI Tests of Lorentz symmetry in the spin-coupling sector SO Special Relativity: Will it Survive the Next 101 years? SE LECTURE NOTES IN PHYSICS LA English DT Proceedings Paper CT 271st WE-Heraeus Seminar on Special Relativity CY FEB 13-18, 2005 CL Potsdam, GERMANY ID HIGHER-DIMENSIONAL THEORIES; HYDROGEN-MASER; ALKALI VAPORS; CPT VIOLATION; STRINGS; EXCHANGE AB An overview is given of recent and ongoing experiments constraining Lorentz violation in the spin-coupling sector, with particular focus on the author's tests of Lorentz symmetry using a Xe-129/He-3 Zeeman maser and an atomic hydrogen maser. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Walsworth, RL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8450 BN 3-540-34522-1 J9 LECT NOTES PHYS PY 2006 VL 702 BP 493 EP 505 DI 10.1007/3-540-34523-X_18 PG 13 WC Physics, Multidisciplinary SC Physics GA BFB86 UT WOS:000240911700018 ER PT S AU Mukhopadhyay, B Afshordi, N Narayan, R AF Mukhopadhyay, Banibrata Afshordi, Niayesh Narayan, Ramesh BE Ghosh, P VandenHeuvel, EPJ TI Growth of hydrodynamic perturbations in accretion disks: Possible route to non-magnetic turbulence SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE accretion; accretion disk; hydrodynamic; turbulence; instabilities ID INSTABILITY; STABILITY; TRANSPORT; BYPASS; FLOW AB We study the possible origin of hydrodynamic turbulence in cold accretion disks such as those in star-forming systems and quiescent cataclysmic variables. As these systems are expected to have neutral gas, the turbulent viscosity is likely to be hydrodynamic in origin, not magnetohydrodynamic. Therefore, MRI will be sluggish or even absent in Such disks. Although there are no exponentially growing eigenmodes in a hydrodynamic disk because of the non-normal nature of the eigenmodes, a large transient growth in the energy is still possible, which may enable the system to switch to a turbulent state. For a Keplerian disk, we estimate that the energy will grow by a factor of 1000 for a Reynolds number close to a million. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Mukhopadhyay, Banibrata; Afshordi, Niayesh; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. RP Mukhopadhyay, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM bmukhopa@cfa.harvard.edu FU NASA [NAG5-10780]; NSF [AST 0307433] FX This work was supported in part by NASA Grant NAG5-10780 and NSF Grant AST 0307433. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 12 BP 2877 EP + DI 10.1016/j.asr.2005.09.048 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600047 ER PT S AU Grindlay, JE AF Grindlay, Jonathan E. BE Ghosh, P VandenHeuvel, EPJ TI Compact X-ray binaries in and out of core collapsed globulars SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE globular clusters; X-rays; general; binaries; close; cataclysmic variables; X-ray biaaries; millisecoad pulsars ID GLOBULAR-CLUSTER-47 TUCANAE; CATACLYSMIC VARIABLES; MILLISECOND PULSARS; CLUSTER; NGC-6397; CHANDRA; POPULATION; CATALOG; STARS; 47TUC AB We review new Chandra and HST observations of the core collapsed cluster NGC 6397 as a guide to understanding the compact binary (CB) populations in core collapse globulars. New cataclysmic variables (CVs) and main sequence chromospherically active binaries (ABs) have been identified, enabling a larger sample for comparison of the L(x), F(x)/F(V), and X-ray vs. optical color distributions. Comparison of the numbers of CBs with L(x) greater than or similar to 10(31) erg s(-1) in 4 core collapse vs. 12 King model Clusters reveals that the specific frequency S(X) (number of CBs per unit cluster mass) is enhanced in core collapse clusters, even when normalized for their stellar encounter rate. Although core collapse is halted by the dynamical heating due to stellar (and binary) interaction with CBs in the core, we conclude that production of the hardest CBs - especially CVs - is enhanced during core collapse. NGC 6397 has its most luminous CVs nearest the cluster center, with two newly discovered very low luminosity (old, quiescent) CVs far from the core. The active binaries as well Lis neutron star systems (MSP and qLMXB) surround the central core. The overall CB population appears to be asymmetric about the cluster center, as in several other core collapse clusters observed with Chandra, suggesting still poorly understood scattering processes. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. 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 20 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 12 BP 2923 EP 2929 DI 10.1016/j.asr.2006.04.027 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600059 ER PT S AU Fabbiano, G AF Fabbiano, G. BE Ghosh, P VandenHeuvel, EPJ TI X-ray populations in galaxies SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE astrophysics; X-ray sources; Chandra; X-ray luminosity functions (XLFs) ID MULTIVARIATE STATISTICAL-ANALYSIS; LUMINOSITY FUNCTION; CHANDRA OBSERVATIONS; SPECTRAL PROPERTIES; STAR-FORMATION; POINT SOURCES; BINARIES; ANTENNAE; EMISSION; INDICATOR AB High-resolution Chandra observations have allowed the detection of populations of X-ray sources in galaxies of all morphological types. The X-ray Luminosity Functions (XLFs) of these X-ray source populations have been derived and studied to uncover the drivers for the formation and evolution of binaries in different stellar populations and environments. These XLFs also provide a tool for identifying the nature of the X-ray source population, since different XLFs characterize X-ray sources belonging to young and old stellar populations. Similarly, X-ray colors can be used for identifying different types of X-ray sources. Ultra-Luminous X-ray sources (ULXs, L(X) > 10(39) ergs s(-1)) are found to be associated with star-forming stellar populations. The study of the ULX population of the Antennae galaxies points to compact accreting binaries. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pepi@cfa.harvard.edu NR 31 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 12 BP 2937 EP 2941 DI 10.1016/j.asr.2006.04.033 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600061 ER PT S AU Kim, DW AF Kim, Dong-Woo BE Ghosh, P VandenHeuvel, EPJ TI LMXB luminosity function and connection to globular cluster in early type galaxies SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE early type galaxies; X-ray; LMXB; globular clusters ID X-RAY BINARIES; ELLIPTIC GALAXIES; CHANDRA OBSERVATIONS; SOURCE POPULATION; MASS; STAR; MULTIWAVELENGTH; INDICATOR AB We derive bias-corrected X-ray luminosity functions (XLFs) of LMXBs detected in 14 E and SO galaxies observed with Chandra. After correcting for incompleteness, the individual XLFs are statistically consistent with a single power-law. A break at or near L(X,Eddington), as previously reported, is not required in any individual case. The combined XLF with a reduced error, however, suggests a possible break at L(X) = 5 x 10(38) erg s(-1), which may be consistent with the Eddington luminosity of neutron stars with the largest possible mass (3 MO), or of He-enriched neutron star binaries. We confirm that the total X-ray luminosity of LNlXBs is correlated with the the near-IR luminosities, but the scatter exceeds that expected from measurement errors. The scatter in L(X)(LMXB)/L(K) appears to be correlated with the specific frequency of globular clusters, as reported earlier. We cross-correlate X-ray binaries with globular clusters determined by ground-based optical and HST observations in 6 giant elliptical galaxies. With the largest sample reported so far (similar to 300 GC LMXBs with a 5:2 ratio between red and blue GCs), we compare their X-ray properties, such as X-ray hardness, XLF and L(X)/L(B) and find no statistically significance difference between different groups of LMXBs. Regardless of their association with GCs, both GC and field LMXBs appear to follow the radial profile of the optical halo light, rather than that of more extended GCs. This suggests that while metallicity is a primary factor in the formation of LNlXBs in GCs, there may be a secondary factor (e.g., encounter rate) playing a non-negligible role. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM kim@cfa.harvard.edu NR 30 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 12 BP 2942 EP 2945 DI 10.1016/j.asr.2006.03.043 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600062 ER PT S AU Zezas, A AF Zezas, Andreas BE Ghosh, P VandenHeuvel, EPJ TI X-ray source populations in nearby star-forming galaxies SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res AB We present results on the X-ray source populations of nearby star-forming galaxies based on Chandra observations. First we discuss the monitoring campaigns on the Antennae and M82 galaxies. In both cases we find that the majority of the X-ray sources exhibit intensity and/or spectral variability. However, despite of this variability, we do not find any statistically significant variations of their X-ray luminosity functions (XLFs). We also find that the majority of the X-ray sources are associated with star-forming regions, although we do not always identify optical counterparts to the X-ray sources. Especially in the case of M82 we find that the most luminous sources are clustered in the central region of the galaxy. Finally, we present the first results from a study of a sample of nearby star-forming galaxies which form a starburst age sequence: although their XLFs to first order are represented by power-laws with consistent slopes, there is an indication for small variations, suggesting a change of their X-ray binary populations. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM azezas@cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 12 BP 2946 EP 2949 DI 10.1016/j.asr.2006.02.070 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600063 ER PT B AU Kallivayalil, N Patten, BM Werner, MW Alcock, C Nguyen, HT AF Kallivayalil, Nitya Patten, Brian M. Werner, Michael W. Alcock, Charles Nguyen, Hien T. BE Armus, L Reach, WT TI Spitzer/IRAC observations of the fields of five LMC microlensing events SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID LARGE-MAGELLANIC-CLOUD; MACHO PROJECT; MACHO-LMC-5; PHOTOMETRY; STARS; DARK AB We have carried out photometry with Spitzer's Infrared Array Camera (IRAC) of five LMC microlensing events in order to look for infrared excesses that would signal that the lenses are dwarf stars that are too cool to have been detected with conventional telescopes thus far. In the case of MACHO-LMC-5, the IRAC fluxes and colors clearly establish that the lens is a M5 dwarf. There is significant excess in the case of MACHO-LMC-4 as well, but with a detection only in I IRAC band, we cannot draw such a clear-cut conclusion for the nature of the candidate lens. For the other three events, we do not detect any infrared excesses. We discuss what these results mean for the microlensing population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kallivayalil, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 70 EP 73 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400012 ER PT B AU Marengo, M Megeath, T Fazio, G Backman, D Stapelfeld, K Werner, M Beichman, C Su, K Stansberry, J Rieke, G AF Marengo, M. Megeath, T. Fazio, G. Backman, D. Stapelfeld, K. Werner, M. Beichman, C. Su, K. Stansberry, J. Rieke, G. BE Armus, L Reach, WT TI Spitzer observations of the debris disk star 6 Eridani SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB epsilon Eridani is one of the four debris disk stars discovered by IRAS (together with Vega, Fomalhaut and beta Pictoris). The disk has been first resolved in the sub-mm, and shows evidences for clumpy structures possibly associated to low mass companions. Radial velocity data also suggest the presence of a planetary companion orbiting at 3.4 AU. With an age of 730 Myr epsilon Eridani represents a particularly interesting object to study the evolution of debris disks and of the associated exoplanetary companions. As part of the Spitzer "Fabulous Four" program, we have observed epsilon Eridani with all Spitzer instruments. In particular, the Multiband Imaging Photometer for Spitzer (MIPS) has been used to image the disk at 24 and 70 mu m, in order to study its infrared thermal emission. The InfraRed Array Camera (IRAC) has instead been used to image the star at 3.6, 4.5, 5.8 and 8.0 mu m in search for substellar companions. We present here the preliminary results of this analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 105 EP 106 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400021 ER PT B AU Hora, JL Latter, WB Marengo, M Fazio, GG Allen, LE Pipher, JL AF Hora, Joseph L. Latter, William B. Marengo, Massimo Fazio, Giovanni G. Allen, Lori E. Pipher, Judith L. BE Armus, L Reach, WT TI IRAC observations of planetary nebulae SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB We present early results from the IRAC imaging survey of planetary nebulae (PNe). The IRAC colors of PNe are red, especially in the 8.0 mu m band. Emission in this band is likely due to contributions from two strong H-2 lines and [Ar III] and [Ne VI] lines in that band. IRAC is sensitive to the emission in the halos as well as in the ionized regions that are optically bright. In NGC 246, we have observed an unexpected ring of emission in the 5.8 and 8.0 mu m IRAC bands not seen previously at other wavelengths. In NGC 650 and NGC 3132, the 8.0 mu m emission is at larger distances from the central star compared to the optical and other TRAC bands, possibly related to the H-2 emission in that band and the tendency for the molecular material to exist outside of the ionized zones. In the flocculi of the outer halo of NGC 6543, however, this trend is reversed, with the 8 mu m emission bright on the inner edges of the structures. This may indicate different emission mechanisms, where the H-2 is possibly excited in shocks in the NGC 6543 halo, whereas the emission is fluorescently excited in the UV fields near the central star in other PNe. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hora, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 144 EP 145 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400030 ER PT B AU Polomski, E Gehrz, RD Woodward, CE Humphreys, RM Boyer, M Brandl, B van Loon, J Fazio, G Willner, SP Barmby, P Ashby, M Pahre, M Rieke, G Gordon, K Hinz, J Engelbracht, C Alonso-Herrero, A Misselt, K Perez-Gonzalez, PG Roellig, T AF Polomski, E. Gehrz, R. D. Woodward, C. E. Humphreys, R. M. Boyer, M. Brandl, B. van Loon, J. Fazio, G. Willner, S. P. Barmby, P. Ashby, M. Pahre, M. Rieke, G. Gordon, K. Hinz, J. Engelbracht, C. Alonso-Herrero, A. Misselt, K. Perez-Gonzalez, P. G. Roellig, T. BE Armus, L Reach, WT TI Multi-epoch imaging and spectroscopy of M33 SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB We have initiated a multi-epoch Spitzer observing campaign of the galaxy M33. The observing program involves mapping the galaxy multiple times over a period of 2.5 years using the IRAC (3-8 mu m) and MIPS (24-160 mu m) cameras and conducting followup IRS spectroscopy of specific sources. The current data set includes IRAC maps from 2003 December, 2004 July, August, and 2005 January, and MIPS maps from 2004 January and 2005 January. These images reveal the entire range of phenomena involved in the creation, evolution, and destruction of dust in star formation regions, evolved stars, and SNR. C1 [Polomski, E.; Gehrz, R. D.; Woodward, C. E.; Humphreys, R. M.; Boyer, M.] Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. [Brandl, B.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Loon, J.] Keele Univ, Sch Chem & Phys, Keele ST5 5BG, Staffs, England. [Fazio, G.; Willner, S. P.; Barmby, P.; Ashby, M.; Pahre, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rieke, G.; Gordon, K.; Hinz, J.; Engelbracht, C.; Alonso-Herrero, A.; Misselt, K.; Perez-Gonzalez, P. G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Roellig, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Polomski, E (reprint author), Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. RI Barmby, Pauline/I-7194-2016; Alonso-Herrero, Almudena/H-1426-2015 OI Barmby, Pauline/0000-0003-2767-0090; Alonso-Herrero, Almudena/0000-0001-6794-2519 NR 3 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 196 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400046 ER PT B AU Surace, JA Wang, Z Willner, S Smith, H Pipher, J Forrest, W Fazio, G AF Surace, J. A. Wang, Z. Willner, S. Smith, H. Pipher, J. Forrest, W. Fazio, G. BE Armus, L Reach, WT TI Spitzer mid-infrared imaging of nearby Ultraluminous Infrared Galaxies SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB We have observed 14 nearby (z < 0.16) Ultraluminous Infrared Galaxies (ULIRGs) with Spitzer at 3.6-24 mu m. The underlying host galaxies are well-detected, in addition to the luminous nuclear cores. While the spatial resolution of Spitzer is poor, the great sensitivity of the data, reveals the underlying galaxy merger remnant, and provides the first look at off-nuclear mid-infrared activity. C1 [Surace, J. A.; Wang, Z.; Willner, S.; Smith, H.; Pipher, J.; Forrest, W.; Fazio, G.] Univ Rochester, Spitzer Sci Ctr, CALTECH, Harvard Smithsonian Ctr Astrophys, Rochester, NY 14627 USA. RP Surace, JA (reprint author), Univ Rochester, Spitzer Sci Ctr, CALTECH, Harvard Smithsonian Ctr Astrophys, Rochester, NY 14627 USA. FU California Institute of Technology under NASA FX JAS was supported by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 1 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 223 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400055 ER PT J AU Chafe, W AF Chafe, Wallace BE Hughes, R TI Reading Aloud SO SPOKEN ENGLISH, TESOL AND APPLIED LINGUISTICS: CHALLENGES FOR THEORY AND PRACTICE LA English DT Article; Book Chapter ID LANGUAGE; WRITTEN C1 [Chafe, Wallace] Univ Calif Berkeley, Berkeley, CA 94720 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Chafe, W (reprint author), Santa Barbara Campus, Santa Barbara, CA USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU PALGRAVE PI BASINGSTOKE PA HOUNDMILLS, BASINGSTOKE RG21 6XS, ENGLAND BN 978-0-230-58458-7 PY 2006 BP 53 EP 71 D2 10.1057/9780230584587 PG 19 WC Education & Educational Research; Language & Linguistics SC Education & Educational Research; Linguistics GA BQD90 UT WOS:000280755600004 ER PT J AU Norman, J AF Norman, Jane TI Lacquer: Technology and conservation: A comprehensive guide to the technology and conservation of Asian and European lacquer SO STUDIES IN CONSERVATION LA English DT Book Review C1 Smithsonian Inst, Freer Gallery Art, Washington, DC 20560 USA. Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU INT INST CONSERVATION HISTORIC ARTISTIC WORKS PI LONDON PA 6 BUCKINGHAM ST, LONDON WC2N 6BA, ENGLAND SN 0039-3630 J9 STUD CONSERV JI Stud. Conserv. PY 2006 VL 51 IS 2 BP 157 EP 158 PG 2 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA 069IQ UT WOS:000239440000008 ER PT J AU Kuntner, M Agnarsson, I AF Kuntner, Matjaz Agnarsson, Ingi TI Are the Linnean and phylogenetic nomenclatural systems combinable? Recommendations for biological nomenclature SO SYSTEMATIC BIOLOGY LA English DT Review ID INCLUSIVE TAXONOMIC UNIT; CROWN CLADES; SPECIES CONCEPTS; CYTOCHROME-B; NAMES; PHYLOCODE; DEFINITION; CLASSIFICATION; ARANEAE; TAXA AB A combination approach between the rules and recommendations from the Linnean (rank-based) and phylogenetic nomenclature is proposed, with a review of the debate. Advantages and drawbacks of both systems are discussed. Too often the debates are biased and unconstructive, and there is a need for dialogue and compromise. Our recommendations for the future of biological classification, to be considered by new editions of all codes of nomenclature, would enable the Linnean and the phylogenetic nomenclatural systems to coexist, or be combined. ( 1) We see it as essential that species binomen, including the formal rank of genus, are retained, and ( 2) species should continue to be linked to type specimens. ( 3) The use of other formal ranks should be minimized; however, we suggest retaining the classical supergeneric ranks ( family, class, order, phylum, kingdom) for purely practical reasons. ( 4) For these ranks and any formally defined clades, type taxa ( species, genera) should be replaced by phylogenetic definitions that explicitly hypothesize monophyly. ( 5) In contrast, species monophyly should not be required, because theory predicts that many species are not monophyletic. ( 6) It should be stressed that equal ranks do not imply comparable evolutionary histories. C1 Slovenian Acad Sci & Arts, Sci Res Ctr, Inst Biol, SI-1001 Ljubljana, Slovenia. Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Sci Res Ctr, Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com; ingi@zoology.ubc.ca NR 118 TC 26 Z9 31 U1 2 U2 9 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYSTEMATIC BIOL JI Syst. Biol. PY 2006 VL 55 IS 5 BP 774 EP 784 DI 10.1080/10635150600981596 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 171FX UT WOS:000246721800006 PM 17060199 ER PT J AU Hacker, BC AF Hacker, BC TI Soldiers and ghosts: A history of battle in classical antiquity. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 2006 VL 47 IS 1 BP 181 EP 182 DI 10.1353/tech.2006.0073 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 030SH UT WOS:000236654200015 ER PT J AU Ceruzzi, P AF Ceruzzi, P TI Jacquard's web: How a hand-loom led to the birth of the information age. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, P (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 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 JAN PY 2006 VL 47 IS 1 BP 197 EP 198 DI 10.1353/tech.2006.0061 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 030SH UT WOS:000236654200024 ER PT J AU Shayt, D AF Shayt, D TI Carriages and clocks, corsets and locks: The rise and fall of an industrial city - New Haven, Connecticut. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Hist, Div Work & Ind, Hand Tool & Engn Collect, Washington, DC 20560 USA. RP Shayt, D (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Work & Ind, Hand Tool & Engn Collect, 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 JAN PY 2006 VL 47 IS 1 BP 213 EP 215 DI 10.1353/tech.2006.0098 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 030SH UT WOS:000236654200034 ER PT J AU Davidson, JF AF Davidson, JF TI Home on the rails: Women, the railroad, and the rise of public domesticity. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 Cape Fear Museum, Wilmington, NC USA. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Davidson, JF (reprint author), Cape Fear Museum, Wilmington, NC 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 JAN PY 2006 VL 47 IS 1 BP 218 EP 219 DI 10.1353/tech.2006.0067 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 030SH UT WOS:000236654200037 ER PT S AU Kimberk, R Hunter, T Tong, CYE Blundell, R AF Kimberk, Robert Hunter, Todd Tong, C. -Y. Edward Blundell, Raymond BE Anwar, M DeMaria, AJ Shur, MS TI Photonic mm-wave local oscillator SO Terahertz Physics, Devices, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Terahertz Physics, Devices, and Systems CY OCT 02-04, 2006 CL Boston, MA SP SPIE DE interferometer; photomixer; phase modulation; phase locked loop; frequency multiplication; millimeter waves AB A millimeter wave source derived from a phase modulated optical signal has been developed. The spectral purity and phase control of the phase of the source allowed it to be used as a local oscillator with an astronomical millimeter wave interferometric array. The phase and amplitude stability of the correlated signals of the array are comparable to that produced by Gunn based local oscillators. The system is explained in the following article first as a simple open loop system and then as a more complex closed loop device where the phase is controlled. A mathematical description is given which predicts system behavior. The telescope correlator output graphs show phase and amplitude stability. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kimberk, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hunter, Todd/0000-0001-6492-0090 NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-6471-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6373 BP U39 EP U45 DI 10.1117/12.686200 PG 7 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BFQ91 UT WOS:000243901900005 ER PT S AU Ryabehun, S Tong, CYE Blundell, R Kimberk, R Gol'tsman, G AF Ryabehun, Sergey Tong, Cheuk-yu Edward Blundell, Raymond Kimberk, Robert Gol'tsman, Gregory BE Anwar, M DeMaria, AJ Shur, MS TI Effect of microwave radiation on the stability of terahertz hot-electron bolometer mixers SO Terahertz Physics, Devices, and Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Terahertz Physics, Devices, and Systems CY OCT 02-04, 2006 CL Boston, MA SP SPIE DE hot-electron bolometer mixers; stability; Allan variance; LO power fluctuations AB We report our studies of the effect of microwave radiation, with a frequency much lower than that corresponding to the energy gap of the superconductor, on the performance of the NbN hot-electron bolometer (HEB) mixer incorporated into a THz heterodyne receiver. It is shown that exposing the HEB mixer to microwave radiation does not result in a significant rise of the receiver noise temperature and degradation of the mixer conversion gain so long as the level of microwave power is small compared to the local oscillator drive. Hence the injection of a small, but controlled amount of microwave radiation enables active compensation of local oscillator power and coupling fluctuations which can significantly degrade the stability of HEB mixer receivers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ryabehun, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Tong, Edward/0000-0002-7736-4203 NR 8 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-6471-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6373 BP U89 EP U93 DI 10.1117/12.686291 PG 5 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BFQ91 UT WOS:000243901900011 ER PT S AU Tong, CYE Kawamura, J Marrone, D Loudkov, D AF Tong, C. -Y. Edward Kawamura, Jonathan Marrone, Daniel Loudkov, Denis BE Anwar, M DeMaria, AJ Shur, MS TI A 1.5 THz hot electron bolometer receiver for ground-based terahertz astronomy in Northern Chile SO TERAHERTZ PHYSICS, DEVICES, AND SYSTEMS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Terahertz Physics, Devices, and Systems CY OCT 02-04, 2006 CL Boston, MA SP SPIE DE terahertz receiver; hot electron bolometer mixer; terahertz astronomy ID SUBMILLIMETER WAVELENGTHS; SPECTROSCOPY; INSTRUMENT; ORION; MIXER; BEAM; COBE AB A 1.5 THz superconducting receiver has been in operation at the Receiver Lab Telescope of the Smithsonian Astrophysical Observatory in Northern Chile since December 2004. This receiver incorporates a Hot Electron Bolometer (HEB) mixer chip made from a thin film of Niobium Titanium Nitride (NbTiN), which is mounted in a precision-machined waveguide mixer block attached to a corrugated waveguide horn assembly. With a noise temperature of around 1500 K, this receiver is sensitive enough for use in the pioneering field of ground-based terahertz spectral-line astronomy. A number of innovative techniques have been employed in the construction and deployment of this receiver. These include near-field vector beam mapping to enable accurate coupling to the telescope optics, the use of tunerless planar-diode based local oscillator unit capable of generating a few mu W at 1.5 THz, and special calibration techniques required for terahertz astronomy. In this paper, we will report on the design, set-up and operation of this state-of-the-art instrument. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Delft Univ Technol, Kavli Inst Nanosci, Delft, Netherlands. OI Tong, Edward/0000-0002-7736-4203; Paine, Scott/0000-0003-4622-5857 NR 28 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-6471-2 J9 PROC SPIE PY 2006 VL 6373 DI 10.1117/12.686058 PG 13 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BFQ91 UT WOS:000243901900019 ER PT S AU McBrearty, S Tryon, C AF McBrearty, Sally Tryon, Christian BE Hovers, E Kuhn, SL TI From Acheulean to Middle Stone Age in the Kapthurin Formation, Kenya SO TRANSITIONS BEFORE THE TRANSITION: EVOLUTION AND STABILITY IN THE MIDDLE PALEOLITHIC AND MIDDLE STONE AGE SE Interdisciplinary Contributions to Archaeology LA English DT Article; Book Chapter ID MODERN HUMAN-BEHAVIOR; MODERN HUMAN ORIGINS; PLEISTOCENE HOMO-SAPIENS; UPPER SEMLIKI VALLEY; SOUTH-AFRICA; HUMAN-EVOLUTION; MODERN HUMANS; BLOMBOS CAVE; EAST-AFRICA; LAND-USE AB The Acheulean to Middle Stone Age (MSA) transition is examined from an evolutionary perspective. The replacement of Acheulean handaxes by MSA points represents a shift from hand-held to hafted technology, but the timing and nature of this process are poorly understood due to the rarity of sites from the early MSA (EMSA), here defined as the portion of the MSA predating 130,000 years ago. The well-calibrated sequence in the Kapthurin Formation, Kenya, spans the transition, and shows that MSA technology was present before 285,000 years ago. This date coincides with the age of known African fossils that most likely represent the earliest members of the Homo sapiens lineage. Occurrences with characteristic Acheulean and EMSA artifacts are interstratified in the Kapthurin Formation, demonstrating that the transition was not a simple, unidirectional process. A variety of flake production techniques is present at both Acheulean and MSA sites in the formation. The Levallois tradition begins before 285,000 BP in an Acheulean context; Levallois production methods diversify in the MSA. The precocious appearance of blades, grindstones, and pigment in the Kapthurin Formation before 285,000 BP shows that the array of sophisticated behaviors known in the later MSA (LMSA) began at the Acheulean to MSA transition, and it is suggested that such technological changes are among the causes or consequences of the origin of our species. C1 [McBrearty, Sally] Univ Connecticut, Dept Anthropol, Storrs, CT 06269 USA. [Tryon, Christian] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP McBrearty, S (reprint author), Univ Connecticut, Dept Anthropol, U-2176, Storrs, CT 06269 USA. NR 130 TC 29 Z9 29 U1 1 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1568-2722 BN 978-0-387-24661-1 J9 INTERD CONTRIB ARCH PY 2006 BP 257 EP 277 DI 10.1007/0-387-24661-4_14 D2 10.1007/b106329 PG 21 WC Archaeology SC Archaeology GA BLK64 UT WOS:000270373600016 ER PT S AU Siebert, L Alvarado, GE Vallance, JW de Vries, BV AF Siebert, Lee Alvarado, Guillermo E. Vallance, James W. de Vries, Benjamin van Wyk BE Rose, WI Bluth, GJS Carr, MJ Ewert, JW Patino, LC Vallance, JW TI Large-volume volcanic edifice failures in Central America and associated hazards SO VOLCANIC HAZARDS IN CENTRAL AMERICA SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE volcano collapse; debris avalanche; hazards; Central America ID DEBRIS AVALANCHE DEPOSITS; CASITA-VOLCANO; AUGUSTINE VOLCANO; MOUNT-RAINIER; EL SALVADOR; COSTA-RICA; COLLAPSE; GUATEMALA; ARC; NICARAGUA AB Edifice-collapse phenomena have, to date, received relatively little attention in Central America, although similar to 40 major collapse events (>= 0.1 km(3)) from about two dozen volcanoes are known or inferred in this volcanic arc. Volcanoes subjected to gravitational failure are concentrated at the arc's western and eastern ends. Failures correlate positively with volcano elevation, substrate elevation, edifice height, volcano volume, and crustal thickness and inversely with slab descent angle. Collapse orientations are strongly influenced by the direction of slope of the underlying basement, and hence are predominately perpendicular to the arc (preferentially to the south) at its extremities and display more variable failure directions in the center of the arc. The frequency of collapse events in Central America is poorly constrained because of the lack of precise dating of deposits, but a collapse interval of similar to 1000-2000 yr has been estimated during the Holocene. These high-impact events fortunately occur at low frequency, but the proximity of many Central American volcanoes to highly populated regions, including some of the region's largest cities, requires evaluation of their hazards. The primary risks are from extremely mobile debris avalanches and associated lahars, which in Central America have impacted now-populated areas up to similar to 50 km from a source volcano. Lower probability risks associated with volcanic edifice collapse derive from laterally directed explosions and tsunamis. The principal hazards of the latter here result from potential impact of debris avalanches into natural or man-made lakes. Much work remains on identifying and describing debris-avalanche deposits in Central America. The identification of potential collapse sites and assessing and monitoring the stability of intact volcanoes is a major challenge for the next decade. C1 [Siebert, Lee] Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, Washington, DC 20013 USA. [Alvarado, Guillermo E.] Inst Costarricense Elect, San Jose, Costa Rica. [Vallance, James W.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. [de Vries, Benjamin van Wyk] Univ Clermont Ferrand, Lab Magmas & Volcans, Observ Phys Globe, Clermont Ferrand, France. RP Siebert, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, MRC 119, Washington, DC 20013 USA. NR 100 TC 11 Z9 11 U1 0 U2 2 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2412-6 J9 GEOL SOC AM SPEC PAP PY 2006 VL 412 BP 1 EP 26 DI 10.1130/2006.2412(01) PG 26 WC Geology; Geosciences, Multidisciplinary SC Geology GA BMG35 UT WOS:000272286100002 ER PT S AU Harris, AJL Vallance, JW Kimberly, P Rose, WI Matias, O Bunzendahl, E Flynn, LP Garbeil, H AF Harris, Andrew J. L. Vallance, James W. Kimberly, Paul Rose, William I. Matias, Otoniel Bunzendahl, Elly Flynn, Luke P. Garbeil, Harold BE Rose, WI Bluth, GJS Carr, MJ Ewert, JW Patino, LC Vallance, JW TI Downstream aggradation owing to lava dome extrusion and rainfall runoff at Volcan Santiaguito, Guatemala SO VOLCANIC HAZARDS IN CENTRAL AMERICA SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE Santiaguito; lava dome; extrusion; lahar; aggradation AB Persistent lava extrusion at the Santiaguito dome complex (Guatemala) results in continuous lahar activity and river bed aggradation downstream of the volcano. We present a simple method that uses vegetation indices extracted from Landsat Thematic Mapper (TM) data to map impacted zones. Application of this technique to a time series of 21 TM images acquired between 1987 and 2000 allow us to map, measure, and track temporal and spatial variations in the area of lahar impact and river aggradation. In the proximal zone of the fluvial system, these data show a positive correlation between extrusion rate at Santiaguito (E), aggradation area 12 months later (A(prox)), and rainfall during the intervening 12 months (Rain(12)): A(prox) = 3.92 + 0.50 E + 0.31 ln(Rain(12)) (r(2) = 0.79). This describes a situation in which an increase in sediment supply (extrusion rate) and/or a means to mobilize this sediment (rainfall) results in an increase in lahar activity (aggraded area). Across the medial zone, we find a positive correlation between extrusion rate and/or area of proximal aggradation and medial aggradation area (A(med)): A(med) = 18.84 - 0.05 A(prox) - 6.15 Rain(12) (r(2) = 0.85). Here the correlation between rainfall and aggradation area is negative. This describes a situation in which increased sediment supply results in an increase in lahar activity but, because it is the zone of transport, an increase in rainfall serves to increase the transport efficiency of rivers flowing through this zone. Thus, increased rainfall flushes the medial zone of sediment. These quantitative data allow us to empirically define the links between sediment supply and mobilization in this fluvial system and to derive predictive relationships that use rainfall and extrusion rates to estimate aggradation area 12 months hence. C1 [Harris, Andrew J. L.; Flynn, Luke P.; Garbeil, Harold] Univ Hawaii, Sch Oceanog & Earth Sci Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Vallance, James W.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. [Kimberly, Paul] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Rose, William I.; Bunzendahl, Elly] Michigan Technol Univ, Dept Geol Engn & Sci, Houghton, MI 49931 USA. [Matias, Otoniel] INSIVUMEH, Guatemala City, Guatemala. RP Harris, AJL (reprint author), Univ Hawaii, Sch Oceanog & Earth Sci Technol, Hawaii Inst Geophys & Planetol, 2525 Correa Rd, Honolulu, HI 96822 USA. EM harris@higp.hawaii.edu NR 21 TC 6 Z9 6 U1 0 U2 1 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2412-6 J9 GEOL SOC AM SPEC PAP PY 2006 VL 412 BP 85 EP 104 DI 10.1130/2006.2412(05) PG 20 WC Geology; Geosciences, Multidisciplinary SC Geology GA BMG35 UT WOS:000272286100006 ER PT S AU Bobbink, R Whigham, DF Beltman, B Verhoeven, JTA AF Bobbink, Roland Whigham, Dennis F. Beltman, Boudewijn Verhoeven, Jos T. A. BE Bobbink, R Beltman, B Verhoeven, JTA Whigham, DF TI Wetland functioning in relation to biodiversity conservation and restoration SO WETLANDS: FUNCTIONING, BIODIVERSITY CONSERVATION, AND RESTORATION SE Ecological Studies-Analysis and Synthesis LA English DT Proceedings Paper CT 7th INTECOL International Wetland Conference CY JUL 25-30, 2004 CL Utrecht, NETHERLANDS SP Utrecht Univ, Landscape Ecol Grp, Int & Natl Sci Comm ID FUTURE C1 [Bobbink, Roland; Beltman, Boudewijn; Verhoeven, Jos T. A.] Univ Utrecht, Inst Environm Biol, POB 800-84, NL-3508 TB Utrecht, Netherlands. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Bobbink, R (reprint author), Univ Utrecht, Inst Environm Biol, POB 800-84, NL-3508 TB Utrecht, Netherlands. EM r.bobbink@bio.uu.nl; whighamd@si.edu; b.beltman@bio.uu.nl; j.t.a.verhoeven@bio.uu.nl RI Verhoeven, Jos/B-9514-2011 NR 10 TC 5 Z9 5 U1 0 U2 22 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0070-8356 BN 3-540-33188-3 J9 ECOL STUD-ANAL SYNTH JI Ecol. Stud. PY 2006 VL 191 BP 1 EP + PG 2 WC Biodiversity Conservation; Ecology; Water Resources SC Biodiversity & Conservation; Environmental Sciences & Ecology; Water Resources GA BFN82 UT WOS:000243355500001 ER PT S AU Barendregt, A Whigham, DF Meire, P Baldwin, AH Van Damme, S AF Barendregt, A. Whigham, D. F. Meire, P. Baldwin, A. H. Van Damme, S. BE Bobbink, R Beltman, B Verhoeven, JTA Whigham, DF TI Wetlands in the tidal freshwater zone SO WETLANDS: FUNCTIONING, BIODIVERSITY CONSERVATION, AND RESTORATION SE Ecological Studies-Analysis and Synthesis LA English DT Proceedings Paper CT 7th INTECOL International Wetland Conference CY JUL 25-30, 2004 CL Utrecht, NETHERLANDS SP Utrecht Univ, Landscape Ecol Grp, Int & Natl Sci Comm ID ESTUARINE SALINITY GRADIENT; DISSOLVED ORGANIC-CARBON; CHESAPEAKE BAY; HUDSON RIVER; SEED-BANK; PHRAGMITES-AUSTRALIS; SCHELDE ESTUARY; DELAWARE-RIVER; SEDIMENT DEPOSITION; SUSPENDED-SEDIMENT C1 [Barendregt, A.] Univ Utrecht, Dept Environm Sci, Copernicus Inst Sustainable Dev & Innovat, POB 80115, NL-3508 TC Utrecht, Netherlands. [Whigham, D. F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Meire, P.; Van Damme, S.] Univ Antwerp, Ecosyst Management Res Grp, Dept Biol, BE-2610 Antwerp, Belgium. [Baldwin, A. H.] Univ Maryland, Dept Biol Resources Engn, College Pk, MD 20742 USA. RP Barendregt, A (reprint author), Univ Utrecht, Dept Environm Sci, Copernicus Inst Sustainable Dev & Innovat, POB 80115, NL-3508 TC Utrecht, Netherlands. EM a.barendregt@geo.uu.nl; whighamd@si.edu; patrick.meire@ua.ac.be; baldwin@umd.edu; stefan.vandamme@ua.ac.be RI Barendregt, Aat/M-1681-2013 OI Barendregt, Aat/0000-0001-6507-8413 NR 128 TC 3 Z9 4 U1 1 U2 5 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0070-8356 BN 3-540-33188-3 J9 ECOL STUD-ANAL SYNTH JI Ecol. Stud. PY 2006 VL 191 BP 117 EP + PG 8 WC Biodiversity Conservation; Ecology; Water Resources SC Biodiversity & Conservation; Environmental Sciences & Ecology; Water Resources GA BFN82 UT WOS:000243355500006 ER PT S AU Greb, SF DiMichele, WA Gastaldo, RA AF Greb, Stephen F. DiMichele, William A. Gastaldo, Robert A. BE Greb, SF DiMichele, WA TI Evolution and importance of wetlands in earth history SO WETLANDS THROUGH TIME SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE paleobotany; paleoecology; paleoflora; earth history; wetlands; coal; swamp; mire; marsh; fen; bog ID CENTRAL APPALACHIAN BASIN; CRETACEOUS-TERTIARY BOUNDARY; PERMIAN-TRIASSIC BOUNDARY; DEVONIAN RHYNIE CHERT; FOREST-NATIONAL-PARK; FOSSIL RECORD; EAST KIRKTON; LAND PLANTS; MIDDLE EOCENE; NORTH-AMERICA AB The fossil record of wetlands documents unique and long-persistent floras and faunas with wetland habitats spawning or at least preserving novel evolutionary characteristics and, at other times, acting as refugia. In addition, there has been an evolution of wetland types since their appearance in the Paleozoic. The first land plants, beginning in the Late Ordovician or Early Silurian, were obligate dwellers of wet substrates. As land plants evolved and diversified, different wetland types began to appear. The first marshes developed in the mid-Devonian, and forest swamps originated in the Late Devonian. Adaptations to low-oxygen, low-nutrient conditions allowed for the evolution of fens (peat marshes) and forest mires (peat forests) in the Late Devonian. The differentiation of wetland habitats created varied niches that influenced the terrestrialization of arthropods in the Silurian and the terrestrialization of tetrapods in the Devonian (and later), and dramatically altered the way sedimentological, hydrological, and various biogeochemical cycles operated globally. Widespread peatlands evolved in the Carboniferous, with the earliest ombrotrophic tropical mires arising by the early Late Carboniferous. Carboniferous wetland-plant communities were complex, and although the taxonomic composition of these wetlands was vastly different from those of the Mesozoic and Cenozoic, these communities were essentially structurally, and probably dynamically, modern. By the Late Permian, the spread of the Glossopteris flora and its adaptations to more temperate or cooler climates allowed the development of mires at higher latitudes, where peats are most common today. Although widespread at the end of the Paleozoic, peat-forming wetlands virtually disappeared following the end-Permian extinction. The initial associations of crocodylomorphs, mammals, and birds with wetlands are well recorded in the Mesozoic. The radiation of Isoetales in the Early Triassic may have included a submerged lifestyle and hence, the expansion of aquatic wetlands. The evolution of heterosporous ferns introduced a floating vascular habit to aquatic wetlands. The evolution of angiosperms in the Cretaceous led to further expansion of aquatic species and the first true mangroves. Increasing diversification of angiosperms in the Tertiary led to increased floral partitioning in wetlands and a wide variety of specialized wetland subcommunities. During the Tertiary, the spread of grasses, rushes, and sedges into wetlands allowed for the evolution of freshwater and salt-water reed marshes. Additionally, the spread of Sphagnum sp. in the Cenozoic allowed bryophytes, an ancient wetland clade, to dominate high-latitude mires, creating some of the most widespread mires of all time. Recognition of the evolution of wetland types and inherent framework positions and niches of both the flora and fauna is critical to understanding both the evolution of wetland functions and food webs and the paleoecology of surrounding ecotones, and is necessary if meaningful analogues are to be made with extant wetland habitats. C1 [Greb, Stephen F.] Univ Kentucky, Kentucky Geol Survey, Lexington, KY 40506 USA. [DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Gastaldo, Robert A.] Colby Coll, Dept Geol, Waterville, ME 04901 USA. RP Greb, SF (reprint author), Univ Kentucky, Kentucky Geol Survey, 228 MMRB, Lexington, KY 40506 USA. NR 427 TC 68 Z9 75 U1 5 U2 28 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2399-0 J9 GEOL SOC AM SPEC PAP PY 2006 VL 399 BP 1 EP 40 DI 10.1130/2006.2399(01) PG 40 WC Geology; Geosciences, Multidisciplinary SC Geology GA BMA33 UT WOS:000271647100002 ER PT S AU DiMichele, WA Tabor, NJ Chaney, DS Nelson, WJ AF DiMichele, William A. Tabor, Neil J. Chaney, Dan S. Nelson, W. John BE Greb, SF DiMichele, WA TI From wetlands to wet spots: Environmental tracking and the fate of Carboniferous elements in Early Permian tropical floras SO WETLANDS THROUGH TIME SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE climate change; paleosols; Permian; tropics; wetlands ID NORTH-CENTRAL TEXAS; TERTIARY PALEOSOLS; LAND PLANTS; NOVA-SCOTIA; WEST TEXAS; NEW-MEXICO; COUNTY; EURAMERICA; TRANSITION; VEGETATION AB Diverse wetland vegetation flourished at the margins of the Midland Basin in north-central Texas during the Pennsylvanian Period. Extensive coastal swamps and an ever-wet, tropical climate supported lush growth of pteridosperm, marattialean fern, lycopsid, and calamite trees, and a wide array of ground cover and vines. As the Pennsylvanian passed into the Permian, the climate of the area became drier and more seasonal, the great swamps disappeared regionally, and aridity spread. The climatic inferences are based on changes in sedimentary patterns and paleosols as well as the general paleobotanical trends. The lithological patterns include a change from a diverse array of paleosols, including Histosols (ever-wet waterlogged soils), in the late Pennsylvanian to greatly diminished paleosol diversity with poorly developed Vertisols by the Early-Middle Permian transition. In addition, coal seams were present with wide areal distribution in the late Pennsylvanian whereas beds of evaporates were common by the end of the Early Permian. During this climatic transition, wetland plants were confined to shrinking "wet spots" found along permanent streams where the vegetation they constituted remained distinct if increasingly depauperate in terms of species richness. By Leonardian (late Early Permian) time, most of the landscape was dominated by plants adapted to seasonal drought and a deep water table. Wetland elements were reduced to scattered pockets, dominated primarily by weedy forms and riparian specialists tolerant of flooding and burial. By the Middle Permian, even these small wetland pockets had disappeared from the region. C1 [DiMichele, William A.; Chaney, Dan S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Tabor, Neil J.] So Methodist Univ, Dept Geol Sci, Dallas, TX 75275 USA. [Nelson, W. John] Illinois State Geol Survey, Champaign, IL 61820 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu; dimichel@si.edu NR 127 TC 56 Z9 58 U1 0 U2 2 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2399-0 J9 GEOL SOC AM SPEC PAP PY 2006 VL 399 BP 223 EP 248 DI 10.1130/2006.2399(11) PG 26 WC Geology; Geosciences, Multidisciplinary SC Geology GA BMA33 UT WOS:000271647100012 ER PT B AU Tagaya, O AF Tagaya, Osamu BE Higham, R Harris, SJ TI The Imperial Japanese Air Forces SO WHY AIR FORCES FAIL: THE ANATOMY OF DEFEAT LA English DT Article; Book Chapter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Tagaya, O (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 34 TC 1 Z9 1 U1 0 U2 0 PU UNIV PRESS KENTUCKY PI LEXINGTON PA 102 LAFFERTY HALL, UNIVERSITY OF KENTUCKY, LEXINGTON, KY 40506 USA BN 978-0-8131-7174-6 PY 2006 BP 177 EP 202 PG 26 WC History SC History GA BAV12 UT WOS:000305581000007 ER PT J AU Kuntner, M AF Kuntner, M TI Phylogenetic systematics of the Gondwanan nephilid spider lineage Clitaetrinae (Araneae, Nephilidae) SO ZOOLOGICA SCRIPTA LA English DT Article ID WEB-BUILDING SPIDERS; ORB-WEAVING SPIDERS; ARANEIDAE; THERIDIIDAE; REVISION; GENUS; ORBICULARIAE; ARANEOIDEA; PLACEMENT; BEHAVIOR AB This study revises the taxonomy, biology, phylogeny, and biogeography of the basal-most nephilid spider lineage, the Clitaetrinae, with the least known nephilid genus Clitaetra. The five previously known species are redescribed: Clitaetra clathrata Simon from western Africa, C. simoni Benoit from central Africa, C. episinoides Simon from the Comoro Islands and Mayotte, C. perroti Simon from Madagascar, and C. thisbe Simon from Sri Lanka with first descriptions of the males of C. clathrata and C. perroti. Additionally, C. irenae sp. nov. is described in both sexes from southern Africa. Clitaetra biology, so far largely unknown, is presented here based on observations of C. irenae in South Africa, and clitaetrine anatomy is summarized to assess phylogenetic homologies. A species-level phylogenetic analysis of 32 taxa scored for 197 morphological and behavioural characters results in eight most parsimonious cladograms and places Clitaetra as sister to the clade (Herennia+ (Nephilengys+Nephila)). Thus, the orb-weaving spider family Nephilidae Simon contains the (sub)tropical genera Nephila, Nephilengys, Herennia, and Clitaetra, but not Deliochus or Phonognatha. Contra recent cladistic treatments, the nephilines are not tetragnathids, but the sister group to the newly proposed clade, Nephilidae, is ambiguous. The three species clades (subgenera) within Clitaetra show a seemingly old Gondwanan biogeographic pattern: Afroetra subgen. nov., with the three mainland African species, is sister to Clitaetra with the two Indian Ocean island species. Indoetra subgen. nov. contains the unstudied species from Sri Lanka, C. thisbe. Future understanding of the morphology and biology of C. thisbe is important for the polarization of many nephilid features. Vicariance would estimate the clitaetrine subgeneric clades and basal nephilid lineages to be at least 160 Myr old and of Gondwanan origin. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com NR 59 TC 58 Z9 63 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 EI 1463-6409 J9 ZOOL SCR JI Zool. Scr. PD JAN PY 2006 VL 35 IS 1 BP 19 EP 62 DI 10.1111/j.1463-6409.2006.00220.x PG 44 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 002ZF UT WOS:000234650400002 ER PT J AU Laurin, M de Queiroz, K Cantino, PD AF Laurin, M de Queiroz, K Cantino, PD TI Sense and stability of taxon names SO ZOOLOGICA SCRIPTA LA English DT Editorial Material ID NOMENCLATURE C1 Univ Paris 07, FRE 2696, F-75005 Paris, France. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. RP Laurin, M (reprint author), Univ Paris 07, FRE 2696, 2 Pl Jussieu, F-75005 Paris, France. EM laurin@ccr.jussieu.fr; dequeirk@si.edu; cantino@ohio.edu RI Laurin, Michel/B-7884-2008 OI Laurin, Michel/0000-0003-2974-9835 NR 11 TC 11 Z9 11 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JAN PY 2006 VL 35 IS 1 BP 113 EP 114 DI 10.1111/j.1463-6409.2006.00219.x PG 2 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 002ZF UT WOS:000234650400007 ER PT J AU Lemaitre, R AF Lemaitre, Rafael TI Two new species of Parapaguridae (Crustacea, Decapoda, Anomura, Paguroidea) with subconical corneas, and new data on biology of some rare species SO ZOOSYSTEMA LA English DT Article DE Crustacea; Decapoda; Anomura; Parapaguridae; Paragiopagurus; Oncopagurus; Typhlopagurus; Bivalvopagurus; hermit crabs; deep-water; misnomers; new species ID SMITH AB Two new parapagurid species with subconical corneas, Oncopagurus conicus n. sp. and Paragiopagurus schnauzer n. sp., are described based on collections by French expeditions to New Caledonia, the Philippines and Solomon Islands, in the western Pacific. These represent the 16th and 18th documented species of Oncopagurus Lemaitre, 1996 and Paragiopagurus Lemaitre, 1996, respectively. Two other parapagurids are known to have subconical corneas, Sympagurus acinops Lemaitre, 1989, and Oncopagurus minutus (Henderson, 1896). Also reported are specimens of two rare and morphologically unique parapagurids, Typhlopagurus foresti de Saint Laurent, 1972 and Bivalvopagurus sinensis (de Saint Laurent, 1972), and represent geographical and bathymetric range extensions for both species. The diagnoses of the monotypic genera Typhlopagurus and Bivalvopagurus are to be modified due to new data on morphology and biology. The former genus was given to include T.foresti, wrongly assumed to lack cornea, thus presumed blind; and the latter for B. sinensis, prematurely assumed to exclusively use bivalve shells as housing. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM lemaitrr@si.edu NR 14 TC 5 Z9 5 U1 0 U2 2 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 J9 ZOOSYSTEMA JI Zoosystema PY 2006 VL 28 IS 2 BP 517 EP 532 PG 16 WC Zoology SC Zoology GA 067RV UT WOS:000239321200024 ER PT J AU Anker, A Caripe, JAV Lira, C AF Anker, Arthur Vera Caripe, Jonathan A. Lira, Carlos TI Description of a new species of commensal alpheid shrimp (Crustacea, Decapoda) from the southern Caribbean Sea SO ZOOSYSTEMA LA English DT Article DE Alpheidae; Leptalpheus; Upogebia; commensal shrimp; infauna; western Atlantic; genus emendation; new species ID GULF-OF-MEXICO; GHOST SHRIMP; THALASSINIDEA; GENUS; CALLIANASSIDAE; LEPIDOPHTHALMUS; CARIDEA; BRAZIL; UPOGEBIIDAE; JAPONICA AB Leptalpheus felderi n. sp., a commensal alpheid Shrimp, is described from two localities in the southern Caribbean Sea: Isla Margarita, Venezuela and Bahia Cispatal Colombia. All specimens of L. felderi n. sp. were collected with the aid of a suction pump; the Venezuelan specimens came from burrows of the upogebiid mudshrimp Upogebia omissa Gomes Correa, 1968. The new species is unique among species of Leptalpheus Williams, 1965 in having small triangular crests on the orbital hoods; a dense row of long, flexible setae on the dactylus of the major chela; two subacute distal processes on the carpus of the major chela; minute, saw-like teeth on the pollex of the minor chela; and only four instead of the usual five segments in the carpus of the second pereiopod. The new species is also characterized by the pinkish-red colour. The diagnosis of the genus Leptalpheus is significantly emended, to accommodate L. felderi n. sp. The taxonomy and intra-generic relationships of Leptalpheus species are discussed, and a table of all species of Leptalpheus, with information on the distribution and hosts, is provided. Because of the invalid description, L. petronii Ramos-Porto & Souza, 1994 is placed in synonymy of L. axianassae Dworschak & Coelho, 1999. Three preliminary species groups, based mainly on the features of the major cheliped and frontal region, are established. C1 Inst Smithsonian Invest Trop, Balboa, Ancon, Panama. Smithsonian Trop Res Inst, APO, AA 34002 USA. Univ Oriente, Isla Margarita, Estado Nueva, Venezuela. RP Anker, A (reprint author), Inst Smithsonian Invest Trop, Balboa, Ancon, Panama. EM ankera@si.edu; j_vera_a_c@yahoo.com; clira@ne.udo.edu.ve NR 48 TC 14 Z9 17 U1 0 U2 0 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 J9 ZOOSYSTEMA JI Zoosystema PY 2006 VL 28 IS 3 BP 683 EP 702 PG 20 WC Zoology SC Zoology GA 100GY UT WOS:000241657500007 ER PT J AU Friedman, M Johnson, GD AF Friedman, M Johnson, GD TI A new species of Mene (Perciformes : Menidae) from the Paleocene of South America, with notes on paleoenvironment SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID PHYLOGENY; FISHES; ACANTHOMORPHS; FORAMINIFERA AB A new species of menid fish, dagger Mene purdyi, is described from northwestern Peru. A Paleocene age (late Thanetian) is estimated for the specimen based on biostratigraphic analysis of planktonic foraminifers recovered from the surrounding matrix. Possible explanations for discrepancies between this result and previous interpretations of an Oligocene age are explored. Stable isotopic analysis of foraminifers associated with the fossil allows for general characterization of the thermal profile of the depositional environment. The small temperature gap between distinct depth-ecological foraminifer assemblages inferred from delta(18)O values indicates a low vertical temperature gradient, possibly reflecting a depositional environment dominated by upwelling. Although incomplete, the three-dimensional preservation of this specimen allows for detailed description of much of the skull, the first two vertebrae and the posttemporals. Numerous characters distinguish the new taxon from previously described menids, the most conspicuous being its exceptionally large size. Comments on the relationships of this new taxon to other menid fishes are premature until the osteology of fossil and living forms are better documented. Extinct species are briefly reviewed in order to facilitate future studies of Menidae. An examination of the distribution of fossil menids reveals that the group was once widespread, demonstrating a circum-global pattern during much of the Tertiary, consistent with the historical Tethys. C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Friedman, M (reprint author), Univ Chicago, Comm Evolutionary Biol, 1025 E 57th St,Culver Hall 402, Chicago, IL 60637 USA. EM mattf@uchicago.edu; johnson.dave@nmnh.si.edu RI Friedman, Matt/F-6991-2012 NR 78 TC 6 Z9 6 U1 0 U2 0 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 DEC 30 PY 2005 VL 25 IS 4 BP 770 EP 783 DI 10.1671/0272-4634(2005)025[0770:ANSOMP]2.0.CO;2 PG 14 WC Paleontology SC Paleontology GA 003PI UT WOS:000234693700003 ER PT J AU Carrano, MT Hutchinson, JR Sampson, SD AF Carrano, MT Hutchinson, JR Sampson, SD TI New information on Segisaurus halli, a small theropod dinosaur from the Early Jurassic of Arizona SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID EXTANT BIRDS NEORNITHES; REPUBLIC-OF-CHINA; MASIAKASAURUS-KNOPFLERI; PREDATORY DINOSAUR; SOFT-TISSUES; EVOLUTION; OSTEOLOGY; HERRERASAURIDAE; MADAGASCAR; MORPHOLOGY AB Here we redescribe the holotype and only specimen of Segisaurus halli, a small Early Jurassic dinosaur and the only theropod known from the Navajo Sandstone. Our study highlights several important and newly recognized features that clarify the relationships of this taxon. Segisaurus is clearly a primitive theropod, although it does possess a tetanuran-like elongate scapular blade. Nonetheless, it appears to be a coelophysoid, based on the presence of a pubic fenestra, a long and ventrally curved pubis, and some pelvic (and possibly tarsal) fusion. Segisaurus does possess a furcula, as has now been observed in other coelophysoids, thus strengthening the early appearance of this 'avian' feature. The absence of an external fundamental system in bone histology sections and the presence of sutural contact lines in the caudal vertebrae, scapulocoracoid, and (possibly) between the pubis and ischium support the inference that this specimen is a subadult. neither a true juvenile nor at full skeletal maturity. A cladistic analysis confirms Segisaurus as a coelophysoid theropod. Poor resolution within Coelophysoidea makes speculation about evolution in this clade difficult, but Segisaurus apparently represents a lineage that had been distinct from Coelophysis and Syntarsus since at least the Carman. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Univ London Royal Vet Coll, Struct & Mot Lab, Hatfield AL9 7TA, Herts, England. Univ Utah, Utah Museum Nat Hist, Salt Lake City, UT 84112 USA. Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA. RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM carranom@si.edu; jrhutch@rvc.ac.uk; ssampson@umnh.utah.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 NR 79 TC 30 Z9 30 U1 0 U2 7 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC 30 PY 2005 VL 25 IS 4 BP 835 EP 849 DI 10.1671/0272-4634(2005)025[0835:NIOSHA]2.0.CO;2 PG 15 WC Paleontology SC Paleontology GA 003PI UT WOS:000234693700008 ER PT J AU Asher, RJ Emry, RJ McKenna, MC AF Asher, RJ Emry, RJ McKenna, MC TI New material of Centetodon (Mammalia, Lipotyphla) and the importance of (missing) DNA sequences in systematic paleontology SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID MOLECULAR-DATA; SUPPORT; TREE; INSECTIVORES; MORPHOLOGY; RESOLUTION; PHYLOGENY; RADIATION; PRIMATES AB We describe new material of the insectivoran genus Centetodon and discuss its anatomy and relationships in the context of recently developed hypotheses of mammalian phylogoeny. Centetodon shows characters common among insectivoran-grade placental mammals, such as an expanded maxillary contribution to the orbital mosaic and relatively small optic foramina. Additional characters such as an enlarged piriform fenestra and a ventrally convex plane of the alveolar maxilla support its position in a clade with extant Holarctic insectivorans (i.e., erinaceids, Solenodon, soricids, and talpids). Our analysis of a combined genetic-morphological matrix supports the recently proposed hypothesis that Solenodon is the basal-most member of a clade of Holarctic insectivorans, including Centetodon and excluding African tenrecoids. Even though DNA sequences are missing for this and most other extinct taxa, they nevertheless help to identify its phylogenetic relationships by better resolving the clades of extant taxa to which it is related. DNA sequences can also influence the topology of fossils by altering the optimization of morphological characters that are known for extinct taxa. The extent of anatomical convergence in Holarctic and African clades of insectivoran-grade mammals is considerable; nevertheless there are diagnostic features that can help determine the affinities of fossil insectivorans with one of these clades. C1 Humboldt Univ, Museum Naturkunde, D-10115 Berlin, Germany. Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Amer Museum Nat Hist, Div Paleontol, Laramie, WY 82071 USA. Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA. RP Asher, RJ (reprint author), Humboldt Univ, Museum Naturkunde, Invalidenstr 43, D-10115 Berlin, Germany. EM robert.asher@museum.hu-berlin.de; Emry.Robert@nmnh.si.edu; m4pmck@indra.com NR 59 TC 15 Z9 16 U1 0 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC 30 PY 2005 VL 25 IS 4 BP 911 EP 923 DI 10.1671/0272-4634(2005)025[0911:NMOCML]2.0.CO;2 PG 13 WC Paleontology SC Paleontology GA 003PI UT WOS:000234693700015 ER PT J AU Thorington, RW Schennum, CE Pappas, LA Pitassy, D AF Thorington, RW Schennum, CE Pappas, LA Pitassy, D TI The difficulties of identifying flying squirrels (Sciuridae : Pteromyini) in the fossil record SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID RODENTIA; PHYLOGENY; EVOLUTION; MAMMALIA; ANATOMY; MIOCENE AB Two problems are examined in this paper: (1) the identification of flying squirrels in the fossil record by means of their teeth; and (2) the identification of features of the limbs that indicate that the animals were gliders. Dental features vary widely among flying squirrels and among other squirrels, and a thorough survey demonstrates that most features that have been used to distinguish fossil flying squirrels are also found in some tree squirrels. A review of the descriptions of fossil flying squirrels reveals few convincing arguments that these animals actually belong to the Ptero-myini and none to support the hypothesis that they were gliding animals. Recent flying squirrels exhibit a number of distinguishing morphological features in their carpal and tarsal bones and at the proximal and distal ends of their long bones. Some of these morphological structures are obligatory features required for gliding locomotion in squirrels and hence are diagnostic of flying squirrels. C1 Smithsonian Inst, Dept Zool, Washington, DC 20560 USA. Virginia Commonwealth Univ, Dept Forens Sci, Richmond, VA 23284 USA. RP Thorington, RW (reprint author), Smithsonian Inst, Dept Zool, Washington, DC 20560 USA. EM Thoringt@si.edu; chad.schennum@dfs.virginia.gov; ldavis@bathpublicschools.com; PitassyD@si.edu NR 43 TC 24 Z9 28 U1 3 U2 17 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 DEC 30 PY 2005 VL 25 IS 4 BP 950 EP 961 DI 10.1671/0272-4634(2005)025[0950:TDOIFS]2.0.CO;2 PG 12 WC Paleontology SC Paleontology GA 003PI UT WOS:000234693700019 ER PT J AU Strong, EE AF Strong, EE TI A morphological reanalysis of Pleurocera acuta Rafinesque, 1831, and Elimia livescens (Menke, 1830) (Gastropoda : Cerithioidea : Pleuroceridae) SO NAUTILUS LA English DT Article ID GONIOBASIS LAQUEATA SAY; LAKE TANGANYIKA; MOLECULAR PHYLOGENY; RDNA SEQUENCES; EAST-AFRICA; CAENOGASTROPODA; PACHYCHILIDAE; PALUDOMIDAE; SYSTEMATICS; VIVIPARITY AB Pleurocera acuta and Elimia livescens have been the subject of several anatomical and ecological studies and are two of the most thoroughly documented species of North American Pleuroceridae. Yet significant gaps still remain in our understanding of their structure. Consequently, the anatomy of these two species is re-described, allowing a re-interpretation of pallial oviduct homologies; features not previously portrayed in the literature (midgut and kidney) are newly described. These taxa are characterized by the presence of an ovipositor, a kidney with a subdivided internal lumen that invades the pallial roof, a prostate with a highly folded anterior spermatophore-forming region, and a pallial oviduct with spermatophore bursa but lacking a seminal receptacle. This analysis verifies the degree of similarity between the two species, but a number of differences were identified including features of the ovipositor, pallial oviduct, prostate, anterior esophagus, midgut, kidney, pericardium and nervous system. Comparison to other pleurocerids confirms that species distributed in Western North America (juga) and Asia (Hua, Semisulcospira) share the presence of a seminal receptacle-a feature that is lacking in all described Eastern North American species. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Strong, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA. EM StrongE@si.edu OI Strong, Ellen/0000-0001-7181-4114 NR 44 TC 14 Z9 14 U1 1 U2 4 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD DEC 30 PY 2005 VL 119 IS 4 BP 119 EP 132 PG 14 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 001IO UT WOS:000234527000001 ER PT J AU Harasewych, MG Kantor, YI AF Harasewych, MG Kantor, YI TI Daffymitra lindae, a new genus and species of Volutomitridae (Neogastropoda) from the Bellingshausen Abyssal Plain SO NAUTILUS LA English DT Article AB Daffymitra lindae, new genus, new species, is described from the Bellingshausen Abyssal Plain off Ellsworthland, Antarctica. Known only from its shell, this new taxon is included in the family Volutomitridae, but differentiated from all known living genera and species on the basis of its inflated shell shape, with an attenuated anterior and distinctive siphonal canal, as well as by the shape and disposition of its three recessed, obliquely oriented columellar plaits. This new taxon represents the first record of Volutomitridae from abyssal depths. The conchological similarity of Daffymitra to the Upper Cretaceous genus Volutomorpha raises the possibility that Daffymitra may be a surviving descendent of a lineage presumed extinct since the end of the Cretaceous, and suggests that a reassessment of the relationships between the various Cretaceous genera assigned to Volutoderminae and the earliest Volutomitridae. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. Russian Acad Sci, Severtzov Inst, Moscow 117071, Russia. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RI Kantor, Yuri/D-5259-2014 OI Kantor, Yuri/0000-0002-3209-4940 NR 13 TC 2 Z9 3 U1 0 U2 0 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD DEC 30 PY 2005 VL 119 IS 4 BP 149 EP 152 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 001IO UT WOS:000234527000003 ER PT J AU Picardi, G Plaut, JJ Biccari, D Bombaci, O Calabrese, D Cartacci, M Cicchetti, A Clifford, SM Edenhofer, P Farrell, WM Federico, C Frigeri, A Gurnett, DA Hagfors, T Heggy, E Herique, A Huff, RL Ivanov, AB Johnson, WTK Jordan, RL Kirchner, DL Kofman, W Leuschen, CJ Nielsen, E Orosei, R Pettinelli, E Phillips, RJ Plettemeier, D Safaeinili, A Seu, R Stofan, ER Vannaroni, G Watters, TR Zampolini, E AF Picardi, G Plaut, JJ Biccari, D Bombaci, O Calabrese, D Cartacci, M Cicchetti, A Clifford, SM Edenhofer, P Farrell, WM Federico, C Frigeri, A Gurnett, DA Hagfors, T Heggy, E Herique, A Huff, RL Ivanov, AB Johnson, WTK Jordan, RL Kirchner, DL Kofman, W Leuschen, CJ Nielsen, E Orosei, R Pettinelli, E Phillips, RJ Plettemeier, D Safaeinili, A Seu, R Stofan, ER Vannaroni, G Watters, TR Zampolini, E TI Radar soundings of the subsurface of Mars SO SCIENCE LA English DT Article ID GEOLOGIC HISTORY; EVOLUTION AB The martian subsurface has been probed to kilometer depths by the Mars Advanced Radar for Subsurface and Ionospheric Sounding instrument aboard the Mars Express orbiter. Signals penetrate the polar layered deposits, probably imaging the base of the deposits. Data from the northern lowlands of Chryse Planitia have revealed a shallowly buried quasi-circular structure about 250 kilometers in diameter that is interpreted to be an impact basin. In addition, a planar reflector associated with the basin structure may indicate the presence of a low-loss deposit that is more than 1 kilometer thick. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy. Alcatel Alenia Space Italia, I-00131 Rome, Italy. Lunar & Planetary Inst, Houston, TX 77058 USA. Ruhr Univ Bochum, Fak Elektrotech & Informat Tech, D-44780 Bochum, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Perugia, Dipartimento Sci Terra, I-06123 Perugia, Italy. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Lab Planetol Grenoble, F-38041 Grenoble, France. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Ist Nazl Astrofis, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Ist Nazl Astrofis, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Univ Rome 3, Dipartimento Fis, I-00146 Rome, Italy. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Tech Univ Dresden, Fak Elektrotech & Informat Tech, D-01062 Dresden, Germany. Proxemy Res, Laytonville, MD 20882 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Plaut, JJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM plaut@jpl.nasa.gov RI Kofman, Wlodek/C-4556-2008; Frigeri, Alessandro/F-2151-2010; Heggy, Essam/E-8250-2013; Farrell, William/I-4865-2013; Ivanov, Anton/C-8944-2014; Herique, Alain/E-7210-2017 OI Frigeri, Alessandro/0000-0002-9140-3977; Heggy, Essam/0000-0001-7476-2735; Ivanov, Anton/0000-0001-8376-8581; Herique, Alain/0000-0003-3699-883X NR 27 TC 159 Z9 166 U1 1 U2 20 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 DEC 23 PY 2005 VL 310 IS 5756 BP 1925 EP 1928 DI 10.1126/science.1122165 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 997UX UT WOS:000234275400034 PM 16319122 ER PT J AU Gingerich, O AF Gingerich, O TI Huygens: The man behind the principle SO NATURE LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 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 DEC 22 PY 2005 VL 438 IS 7071 BP 1083 EP 1084 DI 10.1038/4381083a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 995OF UT WOS:000234111500024 ER PT J AU Rest, A Suntzeff, NB Olsen, K Prieto, JL Smith, RC Welch, DL Becker, A Bergmann, M Clocchiatti, A Cook, K Garg, A Huber, M Miknaitis, G Minniti, D Nikolaev, S Stubbs, C AF Rest, A Suntzeff, NB Olsen, K Prieto, JL Smith, RC Welch, DL Becker, A Bergmann, M Clocchiatti, A Cook, K Garg, A Huber, M Miknaitis, G Minniti, D Nikolaev, S Stubbs, C TI Light echoes from ancient supernovae in the Large Magellanic Cloud SO NATURE LA English DT Article ID SN 1991T; SEARCH; REFLECTIONS; REMNANTS; 1993J AB The light from historical supernovae could in principle still be visible as scattered-light echoes centuries after the explosion(1-6). The detection of light echoes could allow us to pinpoint the supernova event both in position and age and, most importantly, permit the acquisition of spectra to determine the 'type' of the supernova centuries after the direct light from the explosion first reached Earth. Although echoes have been discovered around some nearby extragalactic supernovae(7-13), targeted searches have not found any echoes in the regions of historical Galactic supernovae(14-16). Here we report three faint variable-surface-brightness complexes with high apparent proper motions pointing back to three of the six smallest ( and probably youngest) previously catalogued supernova remnants in the Large Magellanic Cloud, which are believed to have been thermonuclear ( type Ia) supernovae(17). Using the distance and apparent proper motions of these echo arcs, we estimate ages of 610 and 410 years for two of them. C1 Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Gemini Observ, La Serena, Chile. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Suntzeff, NB (reprint author), Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. EM nsuntzeff@ctio.noao.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 NR 25 TC 75 Z9 77 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 DEC 22 PY 2005 VL 438 IS 7071 BP 1132 EP 1134 DI 10.1038/nature04365 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 995OF UT WOS:000234111500044 PM 16372003 ER PT J AU Wcislo, WT AF Wcislo, WT TI Social labels: we should emphasize biology over terminology and not vice versa SO ANNALES ZOOLOGICI FENNICI LA English DT Article ID BEHAVIOR; BEES C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), USA, STRI, Unit 0948, APO, AA 34002 USA. EM wcislow@si.edu NR 20 TC 6 Z9 6 U1 0 U2 7 PU FINNISH ZOOLOGICAL BOTANICAL PUBLISHING BOARD PI UNIV HELSINKI PA P O BOX 17, FIN-00014 UNIV HELSINKI, FINLAND SN 0003-455X J9 ANN ZOOL FENN JI Ann. Zool. Fenn. PD DEC 21 PY 2005 VL 42 IS 6 BP 565 EP 568 PG 4 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 002DV UT WOS:000234592600003 ER PT J AU Pracy, MB Driver, SP De Propris, R Couch, WJ Nulsen, PEJ AF Pracy, MB Driver, SP De Propris, R Couch, WJ Nulsen, PEJ TI Luminosity segregation in three clusters of galaxies (A119, A2443, A2218) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : luminosity function, mass function ID RICH CLUSTERS; COMA CLUSTER; REDSHIFT SURVEY; DWARF GALAXIES; MORPHOLOGY; DISTRIBUTIONS; PHOTOMETRY; DENSITY; CATALOG; FIELD AB We use deep wide-field V-band imaging obtained with the Wide Field Camera at the prime focus of the Issac Newton Telescope to study the spatial and luminosity distribution of galaxies in three low redshift (0.04 < z < 0.2) clusters: Abell 119, Abell 2443 and Abell 2218. The absolute magnitude limits probed in these clusters are M-V- 5 log h(0.7)=-13.3, -15.4 and -16.7 mag, respectively. The galaxy population, at all luminosities, along the line-of-sight to the clusters can be described by the linear combination of a King profile and a constant surface density of field galaxies. We find that, for these three clusters, the core radius is invariant with intrinsic luminosity of the cluster population to the above limits and thus there is no evidence for luminosity segregation in these clusters. The exception is the brightest galaxies in A2218 which exhibit a more compact spatial distribution. We find that the total projected luminosity distribution (within 1 h(0.7)(-1) Mpc of the cluster centre) can be well represented by a single Schechter function with moderately flat faint-end slopes: alpha=-1.22(-0.06)(+0.07) (A119), alpha=-1.11(-0.09)(+0.10)(A2443) and alpha=-1.14(-0.07)(+0.08) (A2218). We perform a geometric deprojection of the cluster galaxy population and confirm that no 'statistically significant' evidence of a change in the shape of the luminosity distribution with cluster-centric radius exists. Again, the exception being A2218 which exhibits a core region with a flatter faint-end slope. C1 Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Australian Natl Univ, Mt Stromlo Observ, Weston, ACT 2611, Australia. Univ Bristol, Astrophys Grp, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pracy, MB (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM mpracy@mso.anu.edu.au RI Driver, Simon/H-9115-2014 OI Driver, Simon/0000-0001-9491-7327 NR 52 TC 20 Z9 21 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 DEC 21 PY 2005 VL 364 IS 4 BP 1147 EP 1157 DI 10.1111/j.1365-2966.2005.09686.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 990XP UT WOS:000233777000003 ER PT J AU Cecchi-Pestellini, C Casu, S Dalgarno, A AF Cecchi-Pestellini, C Casu, S Dalgarno, A TI H-2 excitation in turbulent interstellar clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE molecular processes; turbulence; ISM : clouds; ISM : molecules ID DIFFUSE CLOUDS; COMPARATIVE CHEMISTRY; MOLECULAR-HYDROGEN; PHYSICAL CONDITIONS; BAND SYSTEM; MODELS; PHOTODISSOCIATION; TRANSITION; ABUNDANCES; GAS AB We discuss the observational differences between lines of sight that intercept a group of turbulent dissipative structures and lines of sight that cross less-active regions. Using time-dependent calculations we show that the energy level distribution of the hydrogen molecule evolves in time in response to the local thermal phase. We find that relatively simple models can explain the observed properties of molecular hydrogen in diffuse interstellar clouds in terms of time evolution induced by collisional excitation in a low-density, high-temperature gas. C1 INAF, Osserv Astron Cagliari, I-09012 Capoterra, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cecchi-Pestellini, C (reprint author), INAF, Osserv Astron Cagliari, Str 54 Loc Poggio Pini, I-09012 Capoterra, Italy. EM silvia@galileo.dsf.unica.it OI Cecchi Pestellini, Cesare/0000-0001-7480-0324; Casu, Silvia/0000-0002-0154-3571 NR 43 TC 10 Z9 10 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 DEC 21 PY 2005 VL 364 IS 4 BP 1309 EP 1314 DI 10.1111/j.1365.2005.09652.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 990XP UT WOS:000233777000018 ER PT J AU Brough, S Collins, CA Burke, DJ Lynam, PD Mann, RG AF Brough, S Collins, CA Burke, DJ Lynam, PD Mann, RG TI Environmental dependence of the structure of brightest cluster galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxies : clusters : general; galaxies : elliptical and lenticular; cD; galaxies; evolution; galaxies : formation ID SURFACE BRIGHTNESS TEST; FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; PHOTOMETRIC PROPERTIES; ABSOLUTE MAGNITUDE; LUMINOUS GALAXIES; EXPANSION; UNIVERSE; CATALOG; MERGERS AB We measure the Petrosian structural properties of 33 brightest cluster galaxies (BCGs) at redshifts z <= 0.1 in X-ray selected clusters with a wide range of X-ray luminosities. We find that some BCGs show distinct signatures in their Petrosian profiles, likely to be due to cD haloes. We also find that BCGs in high X-ray luminosity clusters have shallower surface brightness profiles than those in low X-ray luminosity clusters. This suggests that the BCGs in high X-ray luminosity clusters have undergone up to twice as many equal-mass mergers in their past as those in low X-ray luminosity clusters. This is qualitatively consistent with the predictions of hierarchical structure formation. C1 Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago 19001, Chile. Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3NJ, Midlothian, Scotland. RP Brough, S (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. EM sbrough@astro.swin.edu.au OI Burke, Douglas/0000-0003-4428-7835 NR 57 TC 27 Z9 27 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 DEC 21 PY 2005 VL 364 IS 4 BP 1354 EP 1362 DI 10.1111/j.1365-2966.2005.09679.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 990XP UT WOS:000233777000023 ER PT J AU Forman, W Nulsen, P Heinz, S Owen, F Eilek, J Vikhlinin, A Markevitch, M Kraft, R Churazov, E Jones, C AF Forman, W Nulsen, P Heinz, S Owen, F Eilek, J Vikhlinin, A Markevitch, M Kraft, R Churazov, E Jones, C TI Reflections of active galactic nucleus outbursts in the gaseous atmosphere of M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (M87, NGC 4486); X-rays : galaxies ID SPACE-TELESCOPE OBSERVATIONS; XMM-NEWTON OBSERVATIONS; MASSIVE BLACK-HOLE; RAY-EMITTING GAS; X-RAY; COOLING FLOWS; INTRACLUSTER MEDIUM; PERSEUS CLUSTER; VIRGO CLUSTER; RADIO LOBES AB We combined deep Chandra, ROSAT HRI, and XMM-Newton observations of M87 to study the impact of active galactic nucleus (AGN) outbursts on its gaseous atmosphere. Many X-ray features appear to be a direct result of repetitive AGN outbursts. In particular, the X-ray cavities around the jet and counterjet are likely due to the expansion of radio plasma, while rings of enhanced emission at 14 and 17 kpc are probably shock fronts associated with outbursts that began 1-2 x 10(7) yr ago. The effects of these shocks are also seen in brightenings within the prominent X-ray arms. On larger scales, similar to 50 kpc from the nucleus, depressions in the surface brightness may be remnants of earlier outbursts. As suggested for the Perseus Cluster by Fabian and his coauthors, our analysis of the energetics of the M87 outbursts argues that shocks may be the most significant channel for AGN energy input into the cooling-flow atmospheres of galaxies, groups, and clusters. For M87, the mean power driving the shock outburst, 2.4 x 10(43) ergs s(-1), is 3 times greater than the radiative losses from the entire cooling flow. Thus, even in the absence of other energy inputs, outbursts every 3 x 10(7) yr are sufficient to quench the flow. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. MIT, Cambridge, MA 02139 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. Moscow Space Res Inst, IKI, Moscow 117810, Russia. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Forman, W (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wrf@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 NR 61 TC 179 Z9 179 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 894 EP 906 DI 10.1086/429746 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100014 ER PT J AU Hong, J van den Berg, M Schlegel, EM Grindlay, JE Koenig, X Laycock, S Zhao, P AF Hong, J van den Berg, M Schlegel, EM Grindlay, JE Koenig, X Laycock, S Zhao, P TI X-ray processing of ChaMPlane fields: Methods and initial results for selected anti-galactic center fields SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; X-rays : galaxies; X-rays : general ID CHANDRA MULTIWAVELENGTH PROJECT AB We describe the X-ray analysis procedure of the ongoing Chandra Multiwavelength Plane (ChaMPlane) Survey and report the initial results from the analysis of 15 selected anti - Galactic center observations ( 90 degrees < l < 270 degrees). We describe the X-ray analysis procedures for ChaMPlane using custom-developed analysis tools appropriate for Galactic sources but also of general use: optimum photometry in crowded fields using advanced techniques for overlapping sources, rigorous astrometry and 95% error circles for combining X-ray images or matching to optical/ IR images, and application of quantile analysis for spectral analysis of faint sources. We apply these techniques to 15 anti - Galactic center observations ( of 14 distinct fields), in which we have detected 921 X-ray point sources. We present log N-log S distributions and quantile analysis to show that in the hard band ( 2 - 8 keV) active galactic nuclei dominate the sources. Complete analysis of all ChaMPlane anti-Galactic center fields will be given in a subsequent paper, followed by papers on sources in the Galactic center and bulge regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu OI Koenig, Xavier/0000-0002-9478-4170 NR 17 TC 63 Z9 63 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 907 EP 919 DI 10.1086/496966 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100015 ER PT J AU Grindlay, JE Hong, J Zhao, P Laycock, S van den Berg, M Koenig, X Schlegel, EM Cohn, HN Lugger, PM Rogel, AB AF Grindlay, JE Hong, J Zhao, P Laycock, S van den Berg, M Koenig, X Schlegel, EM Cohn, HN Lugger, PM Rogel, AB TI Chandra Multiwavelength Plane (ChaMPlane) survey: An introduction SO ASTROPHYSICAL JOURNAL LA English DT Article DE surveys; X-rays : general ID DIGITAL SKY SURVEY; X-RAY BINARIES; CATACLYSMIC VARIABLES; GALACTIC-CENTER; POINT SOURCES; MILKY-WAY; LUMINOSITY; EMISSION; CATALOG; STARS AB We introduce the Chandra Multiwavelength Plane (ChaMPlane) survey, designed to measure or constrain the populations of low-luminosity (L-X greater than or similar to 10(31) ergs s(-1)) accreting white dwarfs, neutron stars, and stellar mass black holes in the Galactic plane and bulge. ChaMPlane incorporates two surveys, X-ray (Chandra) and optical (NOAO 4 m Mosaic imaging), and a follow-up spectroscopy and IR identification program. The survey has now extended through the first 6 yr of Chandra data using serendipitous sources detected in 105 distinct ACIS-I and ACIS-S fields observed in 154 pointings and covered by 65 deep Mosaic images in V, R, I, and H alpha. ChaMPlane incorporates fields with Galactic latitude vertical bar b vertical bar less than or similar to 12 degrees and selected to be devoid of bright point or diffuse sources, with exposure time greater than or similar to 20 ks and (where possible) minimum N-H. We describe the scientific goals and introduce the X-ray and optical/IR processing and databases. We derive preliminary constraints on the space density or luminosity function of cataclysmic variables (CVs) from the X-ray/optical data for 14 fields in the Galactic anticenter. The lack of ChaMPlane CVs in these anticenter fields suggests that their space density is similar to 3 times below the value ( 3 x 10(-5) pc(-3)) found for the solar neighborhood by previous X-ray surveys. Companion papers describe the X-ray and optical processing in detail, optical spectroscopy of ChaMPlane sources in selected anticenter fields, and IR imaging results for the Galactic center field. An appendix introduces the ChaMPlane Virtual Observatory (VO) for online access to the X-ray and optical images and source catalogs for ready display and further analysis. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@cfa.harvard.edu NR 38 TC 44 Z9 44 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 920 EP 930 DI 10.1086/498106 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100016 ER PT J AU David, LP Jones, C Forman, W Murray, SS AF David, LP Jones, C Forman, W Murray, SS TI The diffuse emission and a variable ultraluminous X-ray point source in the elliptical galaxy NGC 3379 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : elliptical and lenticular, cD; galaxies : individual (NGC 3379); galaxies : ISM; X-rays : binaries; X-rays : galaxies; X-rays : ISM ID GLOBULAR-CLUSTER SYSTEMS; CHANDRA OBSERVATION; SOURCE POPULATION; BLACK-HOLE; BINARIES; COLORS; SCALE; GAS; NGC-4038/4039; PHOTOMETRY AB A Chandra observation of the intermediate-luminosity (M-B = -20) elliptical galaxy NGC 3379 resolves 75% of the X-ray emission within the central 5 kpc into point sources. Spectral analysis of the remaining unresolved emission within the central 770 pc indicates that 90% of the emission probably arises from undetected point sources, while 10% arises from thermal emission from kT 0.6 keV gas. Assuming a uniform density distribution in the central region of the galaxy gives a gas mass of 5 x 10(5) M-circle dot. Such a small amount of gas can be supplied by stellar mass loss in only 10(7) yr. Thus, the gas must be accreting into the central supermassive black hole at a very low radiative efficiency as in the ADAF or RIAFmodels, or it is being expelled in a galactic wind driven by the same AGN feedback mechanism as that observed in cluster cooling flows. If the gas is being expelled in an AGN-driven wind, then the ratio of mechanical to radio power of the AGN must be 104, which is comparable to that measured in cluster cooling flows that have recently been perturbed by radio outbursts. Only 8% of the detected point sources are coincident with globular cluster positions, which is significantly less than that found among other elliptical galaxies observed by Chandra. The low specific frequency of globular clusters and the small fraction of X-ray point sources associated with globular clusters in NGC 3379 is more similar to the properties of lenticular galaxies rather than elliptical galaxies. The brightest point source in NGC 3379 is located 360 pc from the central AGN with a peak luminosity of 3.5 x 10(39) ergs s(-1), which places it in the class of ultraluminous X-ray point sources (ULXs). Analysis of an archival ROSAT HRI observation of NGC 3379 shows that this source was at a comparable luminosity 5 yr prior to the Chandra observation. The spectrum of the ULX is well described by a power-law model with Gamma = 1.6 +/- 0.1 and galactic absorption, similar to other ULXs observed by Chandra and XMM-Newton and to the low-hard state observed in Galactic black hole binaries. During the Chandra observation, the source intensity smoothly varies by a factor of 2 with the suggestion of an 8-10 hr period. No changes in hardness ratio are detected as the intensity of the source varies. While periodic behavior has recently been detected in several ULXs, all of these reside within spiral galaxies. The ULX in NGC 3379 is the only known ULX in an elliptical galaxy with a smoothly varying light curve suggestive of an eclipsing binary system. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM david@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 NR 68 TC 23 Z9 23 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1053 EP 1061 DI 10.1086/497685 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100026 ER PT J AU Keto, E Ho, LC Lo, KY AF Keto, E Ho, LC Lo, KY TI M82, starbursts, star clusters, and the formation of globular clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M82); galaxies : ISM; galaxies : starburst; galaxies : star clusters; ISM : clouds ID SPACE-TELESCOPE OBSERVATIONS; MOLECULAR CLOUDS; MASS FUNCTION; THERMAL INSTABILITIES; DYNAMICAL EVOLUTION; LUMINOSITY FUNCTION; SUPERNOVA-REMNANTS; NUCLEAR STARBURST; ANTENNAE GALAXIES; STELLAR CLUSTERS AB We observed the nearby starburst galaxy M82 in CO in the higher frequency (2 - 1) transition to achieve an angular resolution below 1'' or 17 pc at the target. We resolved the molecular gas into a large number of compact clouds, with masses ranging from similar to 2 x 10(3) to 2 x 10(6) M-circle dot. The mass spectrum scales as N(M) proportional to M-1.5 +/- 0.1, similar to the mass spectra of young massive star clusters, suggesting that individual molecular clouds are transformed in the starburst into individual star clusters. The larger clouds are surrounded by supernovae and H (II) regions, suggesting that star formation proceeds from the outside of the clouds and progresses inward, consistent with triggering by a sudden increase in external pressure. The clouds with internal star formation have velocity gradients and inverse P Cygni spectral line profiles indicating inward motions of 35 km s(-1), consistent with shock-driven compression. Diffuse free-free radio emission and X-ray emission around the clouds provide evidence for superheated ionized gas sufficient to drive the compression. Clouds with spectral lines indicating expansion show little internal star formation, suggesting that the dynamics precedes and is responsible for the star formation rather than the inverse. M82 is known to be in interaction with the neighboring galaxy M81. The overall picture is consistent with the formation of massive star clusters from individual giant molecular clouds crushed by a sudden galactic-scale increase in external pressure generated by the changing dynamics that result from a near-collision with a neighboring galaxy. Present-day globular clusters may have formed in a similar fashion in primordial galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 77 TC 36 Z9 36 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1062 EP 1076 DI 10.1086/497575 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100027 ER PT J AU Keto, E Field, G AF Keto, E Field, G TI Dark cloud cores and gravitational decoupling from turbulent flows SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L1544, B68, L1517B); ISM : molecules; radiative transfer; stars : formation ID MASS STAR-FORMATION; DENSE INTERSTELLAR CLOUDS; CARLO RADIATIVE-TRANSFER; PRE-PROTOSTELLAR CORES; MOLECULAR CLOUD; PRESTELLAR CORES; INFALL MOTIONS; GRAVOTURBULENT FRAGMENTATION; COLLAPSE CANDIDATES; CONTINUUM EMISSION AB We test the hypothesis that the starless cores may be gravitationally bound clouds supported largely by thermal pressure by comparing observed molecular line spectra to theoretical spectra produced by a simulation that includes hydrodynamics, radiative cooling, variable molecular abundance, and radiative transfer in a simple one-dimensional model. The results suggest that the starless cores can be divided into two categories: stable starless cores that are in approximate equilibrium and will not evolve to form protostars, and unstable prestellar cores that are proceeding toward gravitational collapse and the formation of protostars. The starless cores might be formed from the interstellar medium as objects at the lower end of the inertial cascade of interstellar turbulence. In addition, we identify a thermal instability in the starless cores. Under particular conditions of density and mass, a core may be unstable to expansion if the density is just above the critical density for the collisional coupling of the gas and dust so that as the core expands, the gas-dust coupling that cools the gas is reduced and the gas warms, further driving the expansion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 86 TC 42 Z9 42 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 1151 EP 1165 DI 10.1086/497566 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100035 ER PT J AU Akeson, RL Boden, AF Monnier, JD Millan-Gabet, R Beichman, C Beletic, J Calvet, N Hartmann, L Hillenbrand, L Koresko, C Sargent, A Tannirkulam, A AF Akeson, RL Boden, AF Monnier, JD Millan-Gabet, R Beichman, C Beletic, J Calvet, N Hartmann, L Hillenbrand, L Koresko, C Sargent, A Tannirkulam, A TI Keck interferometer observations of classical and weak-line T Tauri stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : protoplanetary disks; stars : pre-main-sequence; techniques : high angular resolution ID HERBIG-AE/BE STARS; MAIN-SEQUENCE EVOLUTION; YOUNG STELLAR OBJECTS; HUBBLE-SPACE-TELESCOPE; DG-TAURI; CIRCUMSTELLAR DISKS; LUNAR OCCULTATION; FORMING REGIONS; IMAGING SURVEY; BINARY STARS AB We present observations of the T Tauri stars BP Tau, DG Tau, DI Tau, GMAur, LkCa 15, RWAur, and V830 Tau, using long baseline infrared interferometry at K band (2.2 mu m) from the Keck Interferometer. The target sources have a range of mass accretion rates and excess near-infrared emission. The interferometer is most sensitive to extended emission on characteristic size scales of 1 - 5 mas. All sources show evidence for resolved K-band emission on these scales, although a few of the sources are marginally consistent with being unresolved. We calculate the infrared excess based on fitting stellar photosphere models to the optical photometry and estimate the physical size of the emission region using simple geometric models for the sources with a significant infrared excess. Assuming that the K-band resolved emission traces the inner edge of the dust disk, we compare the measured characteristic sizes to predicted dust sublimation radii and find that the models require a range of dust sublimation temperatures and possibly optical depths within the inner rim to match the measured radii. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP CALTECH, Michelson Sci Ctr, MS 100-22, Pasadena, CA 91125 USA. NR 72 TC 53 Z9 53 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1173 EP 1181 DI 10.1086/497436 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100037 ER PT J AU Lisse, CM Christian, DJ Dennerl, K Wolk, SJ Bodewits, D Hoekstra, R Combi, MR Makinen, T Dryer, M Fry, CD Weaver, H AF Lisse, CM Christian, DJ Dennerl, K Wolk, SJ Bodewits, D Hoekstra, R Combi, MR Makinen, T Dryer, M Fry, CD Weaver, H TI Chandra observations of comet 2P/Encke 2003: First detection of a collisionally thin, fast solar wind charge exchange system SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : individual (2P/ Encke 2003); solar wind; X-rays : general ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; MULTISCALE MHD MODEL; OUTGASSING ASYMMETRY; IONS; SHOCK; PREDICTIONS; NUCLEUS; ENCKE; SIMULATION AB We report the results of 15 hr of Chandra observations of comet 2P/Encke 2003 on November 24. X-ray emission from comet Encke was resolved on scales of 500-40,000 km, with unusual morphology due to the presence of a low-density, collisionally thin (to charge exchange) coma. A light curve with peak-to-peak amplitude of 20% consistent with a nucleus rotational period of 11.1 hr was found, further evidence for a collisionally thin coma. We confirm emission lines due to oxygen and neon in the 800-1000 eV range but find very unusual oxygen and carbon line ratios in the 200-700 eV range, evidence for low-density, high effective temperature solar wind composition. We compare the X-ray spectral observation results to contemporaneous measurements of the coma and solar wind made by other means and find good evidence for the dominance of a postshock bubble of expanding solar wind plasma, moving at 600 km s(-1) with charge state composition between that of the "fast'' and "slow'' solar winds. C1 Johns Hopkins Univ, Appl Phys Lab, Planetary Exploat Grp, Space Dept, Laurel, MD 20723 USA. Queens Univ Belfast, Dept Pure & Appl Phys, Belfast BT7 1NN, Antrim, North Ireland. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Chandra Xray Observ Ctr, Cambridge, MA 02138 USA. Univ Groningen, NL-9747 AA Groningen, Netherlands. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Finnish Meteorol Inst, Helsinki, Finland. NOAA Space Environm Ctr, Boulder, CO 80305 USA. Explorat Phys Int Inc, Huntsville, AL 35806 USA. RP Johns Hopkins Univ, Appl Phys Lab, Planetary Exploat Grp, Space Dept, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM carey.lisse@jhuapl.edu; d.christian@qub.ac.uk; kod@mpe.mpg.de; swolk@cfa.harvard.edu; bodewits@kvi.nl; hoekstra@kvi.nl; mcombi@engin.umich.edu; teemu.makinen@fmi.fi; murray.dryer@noaa.gov; gfry@expi.com; hal.weaver@jhuapl.edu RI Hoekstra, Ronnie/E-9279-2012; Combi, Michael/J-1697-2012; Weaver, Harold/D-9188-2016; Lisse, Carey/B-7772-2016; OI Combi, Michael/0000-0002-9805-0078; Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020 NR 42 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1329 EP 1347 DI 10.1086/497570 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100052 ER PT J AU Geller, MJ Dell'Antonio, IP Kurtz, MJ Ramella, M Fabricant, DG Caldwell, N Tyson, JA Wittman, D AF Geller, MJ Dell'Antonio, IP Kurtz, MJ Ramella, M Fabricant, DG Caldwell, N Tyson, JA Wittman, D TI SHELS: The hectospec lensing survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : individual (CXOU J092026+302938, CXOU J092053+302800, CXOU J092110+302751); galaxies : distances and redshifts; gravitational lensing; large-scale structure of universe ID LARGE-SCALE STRUCTURE; MASS CORRELATION-FUNCTION; DIGITAL SKY SURVEY; HUBBLE DEEP FIELD; DARK-MATTER; GALAXIES; CLUSTER; COMBO-17; REDSHIFT; LIGHT AB The Smithsonian Hectospec Lensing Survey (SHELS) combines a 10,000 galaxy deep complete redshift survey with a weak-lensing map from the Deep Lens Survey (Wittman et al.). We use maps of the velocity dispersion based on systems identified in the redshift survey to compare the three-dimensional matter distribution with the two-dimensional projection mapped by weak lensing. We demonstrate directly that the lensing map images the three-dimensional matter distribution obtained from the kinematic data. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Brown Univ, Dept Phys, Providence, RI 02912 USA. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; ian@now.het.brown.edu; mkurtz@cfa.harvard.edu; ramella@ts.astro.it; dfabricant@cfa.harvard.edu; ncaldwell@cfa.harvard.edu; tyson@physics.ucdavis.edu; dwittman@physics.ucdavis.edu RI KURTZ, Michael /B-3890-2009; OI Ramella, Massimo/0000-0001-5446-4749; Wittman, David/0000-0002-0813-5888; Kurtz, Michael/0000-0002-6949-0090 NR 42 TC 48 Z9 48 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP L125 EP L128 DI 10.1086/499399 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996OC UT WOS:000234182500004 ER PT J AU Erickson, DL Smith, BD Clarke, AC Sandweiss, DH Tuross, N AF Erickson, DL Smith, BD Clarke, AC Sandweiss, DH Tuross, N TI An Asian origin for a 10,000-year-old domesticated plant in the Americas SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE ancient DNA; archaeology; bottle gourd; domestication ID GOURD LAGENARIA-SICERARIA; BOTTLE GOURD; ANCIENT DNA; CUCURBITACEAE; DIVERSITY AB New genetic and archaeological approaches have substantially improved our understanding of the transition to agriculture, a major turning point in human history that began 10,000-5,000 years ago with the independent domestication of plants and animals in eight world regions. In the Americas, however, understanding the initial domestication of New World species has long been complicated by the early presence of an African enigma, the bottle gourd (Lagenaria siceraria). Indigenous to Africa, it reached East Asia by 9,000-8,000 before present (B.P.) and had a broad New World distribution by 8,000 B.P. Here we integrate genetic and archaeological approaches to address a set of long-standing core questions regarding the introduction of the bottle gourd into the Americas. Did it reach the New World directly from Africa or through Asia? Was it transported by humans or ocean currents? Was it wild or domesticated upon arrival? Fruit rind thickness values and accelerator mass spectrometer radiocarbon dating of archaeological specimens indicate that the bottle gourd was present in the Americas as a domesticated plant by 10,000 B.P., placing it among the earliest domesticates in the New World. Ancient DNA sequence analysis of archaeological bottle gourd specimens and comparison with modern Asian and African landraces identify Asia as the source of its introduction. We suggest that the bottle gourd and the dog, two "utility" species, were domesticated long before any food crops or livestock species, and that both were brought to the Americas by Paleoindian populations as they colonized the New World. C1 Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20560 USA. Massey Univ, Allan Wilson Ctr Mol Ecol & Evolut, Palmerston North 5301, New Zealand. Massey Univ, Inst Mol Biosci, Palmerston North 5301, New Zealand. Univ Maine, Dept Anthropol, Orono, ME 04469 USA. Harvard Univ, Dept Anthropol, Cambridge, MA 02138 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. EM smithb@si.edu RI Clarke, Andrew/A-7635-2008 OI Clarke, Andrew/0000-0003-2293-1423 NR 38 TC 90 Z9 96 U1 3 U2 27 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 DEC 20 PY 2005 VL 102 IS 51 BP 18315 EP 18320 DI 10.1073/pnas.0509279102 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 996LB UT WOS:000234174300015 PM 16352716 ER PT J AU Petit, RE Harasewych, MG AF Petit, RE Harasewych, MG TI Catalogue of the superfamily Cancellarioidea Forbes and Hanley, 1851 (Gastropoda : Prosobranchia) - 2nd edition SO ZOOTAXA LA English DT Review DE Cancellarioidea; genus-list; species-list; bibliography ID SOUTH-AFRICA; MOLLUSCA; NEOGASTROPODA; FAUNA; GENUS; TAXA AB This catalogue of cancellarioidean taxa is composed of three sections. The first lists alphabetically 124 genus-group taxa originally proposed or later included within the superfamily as well as 24 misspelled or nude names. The second section lists alphabetically 1,864 species-group names proposed in or subsequently referred to genera now considered to belong in Cancellarioidea. Also listed are 392 nude names, misspellings and incorrect attributions. The third section consists of a bibliography of works referred to in this paper. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Petit, RE (reprint author), 806 St Charles Rd, N Myrtle Beach, SC 29582 USA. EM r.e.petit@att.net; harasewych@si.edu NR 919 TC 10 Z9 11 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD DEC 19 PY 2005 IS 1102 BP 1 EP 161 PG 161 WC Zoology SC Zoology GA 994CD UT WOS:000234006700001 ER PT J AU Shim, C Wang, YH Choi, Y Palmer, PI Abbot, DS Chance, K AF Shim, C Wang, YH Choi, Y Palmer, PI Abbot, DS Chance, K TI Constraining global isoprene emissions with Global Ozone Monitoring Experiment (GOME) formaldehyde column measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ORGANIC-COMPOUND EMISSIONS; NORTH-AMERICA; NONMETHANE HYDROCARBONS; TROPOSPHERIC CHEMISTRY; SATELLITE-OBSERVATIONS; OH; IMPACT; SPACE; MODEL; PHOTOOXIDATION AB Biogenic isoprene plays an important role in tropospheric chemistry. Current isoprene emission estimates are highly uncertain because of a lack of direct observations. Formaldehyde (HCHO) is a high-yield product of isoprene oxidation. The short photochemical lifetime of HCHO allows the observation of this trace gas to help constrain isoprene emissions. We use HCHO column observations from the Global Ozone Monitoring Experiment (GOME). These global data are particularly useful for studying large isoprene emissions from the tropics, where in situ observations are sparse. Using the global Goddard Earth Observing System-Chemistry (GEOS-CHEM) chemical transport model as the forward model, a Bayesian inversion of GOME HCHO observations from September 1996 to August 1997 is conducted to calculate global isoprene emissions. Column contributions to HCHO from 10 biogenic sources, in addition to biomass-burning and industrial sources, are considered. The inversion of these 12 HCHO sources is conducted separately for eight geographical regions (North America, Europe, east Asia, India, Southeast Asia, South America, Africa, and Australia). GOME measurements with high signal-to-noise ratios are used. The a priori simulation greatly underestimates global HCHO columns over the eight geographical regions (bias, -14 to -46%; R=0.52-0.84). The a posteriori solution shows generally higher isoprene and biomass-burning emissions, and these emissions reduce the model biases for all regions (bias, -3.6 to -25%; R=0.56-0.84). The negative bias in the a posteriori estimate reflects in part the uncertainty in GOME measurements. The a posteriori estimate of the annual global isoprene emissions of 566 Tg C yr(-1) is similar to 50% larger than the a priori estimate. This increase of global isoprene emissions significantly affects tropospheric chemistry, decreasing the global mean OH concentration by 10.8% to 0.95x10(6) molecules/cm(3). The atmospheric lifetime of CH3CCl3 increases from 5.2 to 5.7 years. C1 Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Georgia Inst Technol, Dept Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM cshim@eas.gatech.edu RI Palmer, Paul/F-7008-2010; Abbot, Dorian/J-6352-2012; Wang, Yuhang/B-5578-2014; Chem, GEOS/C-5595-2014 NR 44 TC 76 Z9 76 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2005 VL 110 IS D24 AR D24301 DI 10.1029/2004JD005629 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 998BW UT WOS:000234293900002 ER PT J AU Torres-Mejia, M Vari, RP AF Torres-Mejia, M Vari, RP TI New species of Creagrutus (Teleostei : Characiformes : Characidae) from the Rio Magdalena basin, Colombia SO COPEIA LA English DT Article ID BRAZIL AB A new species of Creagrutus from the Rio Magdalena basin, Colombia, is described. This species is distinguished from all congeners by a combination of morphometric, meristic, and morphological features. The species is the first member of the genus known to have breeding tubercles with keratinized caps. The phylogenetic position of the new species and various aspects of its ecology and behavior are discussed. C1 Univ Ind Santander, Lab Biol Reprod Vertebrados, Grp Estudios Biodiversidad, Bucaramanga 678, Colombia. Smithsonian Inst, Div Fisheries, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Vari, RP (reprint author), Univ Ind Santander, Lab Biol Reprod Vertebrados, Grp Estudios Biodiversidad, Bucaramanga 678, Colombia. EM mauricio_4iiik@yahoo.com; vari.richard@nmnh.si.edu NR 11 TC 6 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 DEC 15 PY 2005 IS 4 BP 812 EP 817 PG 6 WC Zoology SC Zoology GA 995GF UT WOS:000234088100010 ER PT J AU Mohamed, S McCarthy, MC Cooksy, AL Hinton, C Thaddeus, P AF Mohamed, S McCarthy, MC Cooksy, AL Hinton, C Thaddeus, P TI Rotational spectra of the carbon-chain radicals HC5O, HC6O, and HC7O SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID HYPERFINE-STRUCTURE; MICROWAVE SPECTROSCOPY; PARAMETERS; MOLECULES; HCCCO; HCO AB Three new free carbon-chain radicals, HC5O, HC6O, and HC7O, and their deuterated isotopic species have been observed by Fourier transform microwave spectroscopy of a supersonic molecular beam. In contrast to the shorter HCnO radicals, these all have linear heavy-atom backbones and (2)Pi electronic ground states. Like the isovalent HCnS radicals, the ground states of the HCnO radicals alternate with odd and even numbers of carbon atoms: those of HC5O and HC7O are (2)Pi(1/2) and that of HC6O is (2)Pi(3/2). From frequency measurements between 6 and 26 GHz, the rotational constant B, the centrifugal distortion constant D, and the lambda-type doubling and magnetic hyperfine constants have been determined to high precision for each chain. Predicted properties from coupled-cluster calculations are also reported for chains up to HC9O. The production of HCnO radicals for n even was highly favored when O-2 was used as the source of oxygen, but those with n odd were best produced with CO. (c) 2005 American Institute of Physics. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. San Diego State Univ, Dept Chem, San Diego, CA 92182 USA. RP Mohamed, S (reprint author), Univ Utah, Dept Chem, Salt Lake City, UT 84112 USA. EM mccarthy@cfa.harvard.edu NR 27 TC 8 Z9 8 U1 2 U2 6 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 DEC 15 PY 2005 VL 123 IS 23 AR 234301 DI 10.1063/1.216970 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 996AD UT WOS:000234145900012 PM 16392914 ER PT J AU Kharchenko, V Dalgarno, A Fox, JL AF Kharchenko, V Dalgarno, A Fox, JL TI Thermospheric distribution of fast O(D-1) atoms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SCHUMANN-RUNGE CONTINUUM; POTENTIAL-ENERGY SURFACE; HOT OXYGEN GEOCORONA; FAST NITROGEN-ATOMS; DISSOCIATIVE RECOMBINATION; QUANTUM YIELDS; TRANSLATIONAL ENERGY; O(1D) ATOMS; AE-E; COLLISIONAL EXCITATION AB [1] Detailed calculations are carried out of the sources of energetic metastable O(D-1) atoms in the atmosphere at altitudes between 80 km and 200 km, and the corresponding energy distribution functions are derived, taking account of energy transfer and quenching in collisions of the metastable atoms with the ambient atmospheric gas constituents. The energy relaxation of metastable oxygen atoms produced by O-2 and O-3 photolysis and O-2(+) dissociative recombination is determined by solving the time-dependent Boltzmann equation. The O(D-1) thermalization and quenching times are obtained as functions of the altitude. The steady state distributions of metastable O(D-1) are computed and used for the determination of the parameters characterizing the nonthermal O(D-1) atoms. The nonthermal atoms comprise 4 - 6% of the distribution, and their effective temperatures are larger by 25 - 46% than the local temperatures of the ambient gas. The role of hot metastable oxygen atoms in the production of vibrationally excited OH molecules is analyzed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Wright State Univ, Dept Phys, Dayton, OH 45435 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vkharchenko@cfa.harvard.edu NR 79 TC 12 Z9 12 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-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2005 VL 110 IS A12 AR A12305 DI 10.1029/2005JA011232 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CR UT WOS:000234296100006 ER PT J AU Renner, SC AF Renner, SC TI Biodiversity: there's a role to be played by 'museum-keepers' too SO NATURE LA English DT Letter C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Renner, SC (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. OI Renner, Swen/0000-0002-6893-4219 NR 1 TC 1 Z9 1 U1 0 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 15 PY 2005 VL 438 IS 7070 BP 914 EP 914 DI 10.1038/438914a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 993EC UT WOS:000233934600028 PM 16355192 ER PT J AU Babich, D Loeb, A AF Babich, D Loeb, A TI Polarization of 21 cm radiation from the epoch of reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; intergalactic medium; polarization; radio lines : general ID LARGE-SCALE STRUCTURE; MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; COSMIC MAGNETIC-FIELDS; HIGH-REDSHIFT; CENTIMETER FLUCTUATIONS; INTERGALACTIC MEDIUM; NEUTRAL HYDROGEN; TOMOGRAPHY; GALAXIES AB We consider the polarization of 21 cm line radiation from the epoch of reionization due to both intrinsically polarized emission and secondary mechanisms. We argue that Thomson scattering of the 21 cm quadrupole by the reionized universe is likely to produce the largest effect. The 21 cm quadrupole is sourced by baryonic density fluctuations and the fluctuations in the ionization fraction due to discrete H II regions. Since Thomson scattering produces only E-type polarization and is achromatic, its unique fingerprint could in principle be separated from foregrounds associated with polarized synchrotron emission, which should not be correlated with the cosmic signal. We estimate that Poisson fluctuations of H II regions at the end of reionization (z(R) similar to 6-20) produce a brightness temperature-polarization cross-correlation signal of similar to 0.1-0.3 mK on angular scales of tens of arcminutes. This cross-correlation signal is within the instrument sensitivities of the future Square Kilometre Array (SKA) and close to the sensitivities of the forthcoming Mileura Widefield Array (MWA) and Low Frequency Array (LOFAR). 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, 17 Oxford St, Cambridge, MA 02138 USA. EM babich@physics.harvard.edu; aloeb@cfa.harvard.edu NR 54 TC 10 Z9 10 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2005 VL 635 IS 1 BP 1 EP 10 DI 10.1086/497297 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600001 ER PT J AU Keeton, CR Gaudi, BS Petters, AO AF Keeton, CR Gaudi, BS Petters, AO TI Identifying lenses with small-scale structure. II. Fold lenses SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; dark matter; galaxies : formation; gravitational lensing; large-scale structure of universe ID DARK-MATTER SUBSTRUCTURE; OPTICAL EINSTEIN RING; 4-IMAGE GRAVITATIONAL LENS; EMISSION-LINE REGION; EARLY-TYPE GALAXIES; QUADRUPLE LENSES; EXTERNAL SHEAR; PG 1115+080; QUINTUPLE QUASAR; MERGER REMNANTS AB When the source in a four-image gravitational lens system lies sufficiently close to a "fold'' caustic, two of the lensed images lie very close together. If the lens potential is smooth on the scale of the separation between the two close images, the difference between their fluxes should approximately vanish, R-fold equivalent to (F+ - F-)/(F+ + F-) approximate to 0. ( The subscript indicates the image parity.) Violations of this "fold relation'' in observed lenses are thought to indicate the presence of structure on scales smaller than the separation between the close images. We present a detailed study of the fold relation in realistic smooth lenses, finding it to be more subtle and rich than was previously realized. The degree to which R-fold can differ from zero for smooth lenses depends not only on the distance of the source from the caustic, but also on its location along the caustic, and then on the angular structure of the lens potential (ellipticity, multipole modes, and external shear). Since the source position is unobservable, it is impossible to say from R-fold alone whether the flux ratios in an observed lens are anomalous or not. Instead, we must consider the full distribution of R-fold values that can be obtained from smooth lens potentials that reproduce the separation d(1) between the two close images and the distance d(2) to the next nearest image. (By reducing the image configuration to these two numbers, we limit our model dependence and obtain a generic analysis.) We show that the generic features of this distribution can be understood, which means that the fold relation provides a robust probe of small-scale structure in lens galaxies. We then compute the full distribution using Monte Carlo simulations of realistic smooth lenses. Comparing these predictions with the data, we find that five of the 12 known lenses with fold configurations have flux ratio anomalies: B0712+472, SDSS0924+0219, PG1115+080, B1555+375, and B1933+503. Combining this with our previous analysis revealing anomalies in three of the four known lenses with cusp configurations, we conclude that at least half (8/16) of all four-image lenses that admit generic, local analyses exhibit flux ratio anomalies. The fold and cusp relations do not reveal the nature of the implied small-scale structure, but do provide the formal foundation for substructure studies, and also indicate which lenses deserve further study. Although our focus is on close pairs of images, we show that the fold relation can be used - with great care - to analyze all image pairs in all 22 known four-image lenses and reveal lenses with some sort of interesting structure. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08837 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Duke Univ, Dept Math, Durham, NC 27708 USA. Duke Univ, Dept Phys, Durham, NC 27708 USA. RP Keeton, CR (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08837 USA. EM keeton@physics.rutgers.edu; sgaudi@cfa.harvard.edu; petters@math.duke.edu RI Gaudi, Bernard/I-7732-2012 NR 99 TC 48 Z9 48 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 35 EP 59 DI 10.1086/497324 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600004 ER PT J AU Cen, RY Nagamine, K Ostriker, JP AF Cen, RY Nagamine, K Ostriker, JP TI Quantitative signatures of galactic superwinds on Ly alpha clouds and metal-line systems SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; hydrodynamics; intergalactic medium; large-scale structure of universe; quasars : absorption lines ID COLD DARK-MATTER; X-RAY-CLUSTERS; SMOOTHED-PARTICLE HYDRODYNAMICS; HOT INTERGALACTIC MEDIUM; LYMAN-BREAK GALAXIES; ON STARBURST GALAXIES; MASS INJECTION RATES; LARGE-SCALE WINDS; HIGH-REDSHIFT; COSMOLOGICAL SIMULATIONS AB We investigate possible signatures of feedback from galactic superwinds (GSWs) on the metallicity of the Ly alpha forest, using a set of high-resolution hydrodynamic simulations of a Lambda CDM model. Simulations produce metals self-consistently, based on one single parameter, the metal yield, which in turn is constrained by metallicity in the intracluster gas. We follow metals as a separate density species. The metallicity of Ly alpha clouds having column density of N(H I) similar to 10(14.5)-10(15.5) cm(-2) at z = 2-4 is correctly predicted by simulations, both with and without GSWs, implying an in situ origin for these metals. However, a unique signature and sensitive test of GSWs are provided by lower column density clouds of 10(12)-10(14) cm(-2). We find that the number density of Ly alpha lines with metallicity Z >= 10(-3) Z circle dot and neutral hydrogen column density N(H I) < 10(13.5) cm(-2) provides a first quantitative measure of the strength of GSWs, because metals in these systems are a contaminant. We predict that the number of such lines per unit redshift at z similar to 3 should be about 0.1 in the absence of GSWs. With the observed GSW strength, we expect to see 20-50 such lines per unit redshift. This is an observational challenge. Furthermore, we find that the difference between simulations with and without GSWs becomes much larger with regard to a subset of such clouds with high Doppler widths, since the contaminated systems are considerably hotter than the normal IGM. We also present preliminary results on C IV and O vi lines as a function of GSW strength. The filling factor of metal-rich regions is a strong function of GSWs. With and without GSWs the volume filling factor is 6.0%, 4.2%, and 1.9% and 1.0%, 0.28%, and 0.08%, respectively, for regions with metallicity greater than 10(-3), 10(-2), and 10(-1) Z circle dot. Finally, in clouds of N(H) I similar to 10(14.5) cm(-2), we predict that the ratio of secondary ( e. g., N) to primary metals ( e. g., O, C) is expected to be smaller by a factor of 10 than in large galaxies, which better retain metals; this factor increases to >= 50 for N(H I) <= 10(13.5) cm(-2). C1 Princeton Univ, Princeton Univ Observ, Princeton, NJ 08544 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cen, RY (reprint author), Princeton Univ, Princeton Univ Observ, Princeton, NJ 08544 USA. EM cen@astro.princeton.edu; knagamin@cfa.harvard.edu; jpo@astro.princeton.edu NR 132 TC 65 Z9 65 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 86 EP 99 DI 10.1086/497353 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600007 ER PT J AU Wang, QD Yao, Y Tripp, TM Fang, TT Cui, W Nicastro, F Mathur, S Williams, RJ Song, L Croft, R AF Wang, QD Yao, Y Tripp, TM Fang, TT Cui, W Nicastro, F Mathur, S Williams, RJ Song, L Croft, R TI Warm-hot gas in and around the Milky Way: Detection and implications of OVII absorption toward LMC X-3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE intergalactic medium; ISM : kinematics and dynamics; stars : individual (LMC X-3); techniques : spectroscopic; ultraviolet : ISM; X-rays : ISM ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; X-RAY FOREST; HIGH-VELOCITY CLOUDS; LARGE-MAGELLANIC-CLOUD; O-VI ABSORPTION; INTERSTELLAR-MEDIUM; INTERGALACTIC MEDIUM; LMC X-3; LOW-REDSHIFT; GALACTIC HALO AB X-ray absorption lines of highly ionized species such as O VII at about zero redshift have been firmly detected in the spectra of several active galactic nuclei. However, the location of the absorbing gas remains a subject of debate. To separate the Galactic and extragalactic contributions to the absorption, we have obtained Chandra LETG-HRC and Far Ultraviolet Spectroscopic Explorer observations of the black hole X-ray binary LMC X-3. We clearly detect the O VII K alpha absorption line with an equivalent width of 20(14, 26) m angstrom (90% confidence range). The Ne IX K alpha absorption line is also detected, albeit marginally. A joint analysis of these lines, together with the nondetection of the O VII K beta and O VIII K alpha lines, gives the temperature, velocity dispersion, and hot oxygen column density as 1.3(0.7, 1.8); 10(6) K, 79(62,132) km s(-1), and 1.9(1.2, 3.2) x 10(16) cm(-2), assuming a collisional ionization equilibrium of the X-ray-absorbing gas and a Galactic interstellar Ne/O number ratio of 0.18. The X-ray data allow us to place a 95% confidence lower limit to the Ne/O ratio as 0.14, but the upper limit is not meaningfully constrained. The O VII line centroid and its relative shift from the Galactic O I K alpha absorption line, detected in the same observations, are inconsistent with the systemic velocity of LMC X-3 (+310 km s(-1)). The far-UV spectrum shows O VI absorption at Galactic velocities, but no O VI absorption is detected at the LMC velocity at greater than 3 sigma significance. The measured Galactic O VI column density is higher than the value predicted from the O VII-bearing gas, indicating multiphase absorption. Both the nonthermal broadening and the decreasing scale height with the increasing ionization state further suggest an origin of the highly ionized gas in a supernova-driven galactic fountain. In addition, we estimate the warm and hot electron column densities from our detected O II K alpha line in the LMC X-3 X-ray spectra and from the dispersion measure of a pulsar in the LMC vicinity. We then infer the O/H ratio of the gas to greater than or similar to 8 x 10(-5), consistent with the chemically enriched galactic fountain scenario. We conclude that the Galactic hot interstellar medium should in general substantially contribute to zero-redshift X-ray absorption lines in extragalactic sources. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Wang, QD (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM wqd@astro.umass.edu; yaoys@astro.umass.edu RI Croft, Rupert/N-8707-2014; OI Croft, Rupert/0000-0003-0697-2583; Cui, Wei/0000-0002-6324-5772; Nicastro, Fabrizio/0000-0002-6896-1364 NR 63 TC 60 Z9 60 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 386 EP 395 DI 10.1086/497584 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600031 ER PT J AU Boden, AF Sargent, AI Akeson, RL Carpenter, JM Torres, G Latham, DW Soderblom, DR Nelan, E Franz, OG Wasserman, LH AF Boden, AF Sargent, AI Akeson, RL Carpenter, JM Torres, G Latham, DW Soderblom, DR Nelan, E Franz, OG Wasserman, LH TI Dynamical masses for low-mass pre-main-sequence stars: A preliminary physical orbit for HD 98800 B SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : fundamental parameters; stars : individual (HD 98800); stars : pre-main sequence ID STANDARD STELLAR LIBRARY; T-TAURI STARS; HD 98800; EVOLUTIONARY SYNTHESIS; VISUAL ORBIT; SYSTEM; TRACKS; DISK; CIRCUMSTELLAR; CONSTRAINTS AB We report on Keck Interferometer observations of the double-lined binary ( B) component of the quadruple pre-main-sequence (PMS) system HD 98800. With these interferometric observations, combined with astrometric measurements made by the Hubble Space Telescope (HST) Fine Guidance Sensors (FGS) and published radial velocity observations, we have estimated preliminary visual and physical orbits of the HD 98800 B subsystem. Our orbit model calls for an inclination of 66.degrees 8 +/- 3.degrees 2 and allows us to infer the masses and luminosities of the individual components. In particular we find component masses of 0.699 +/- 0.064 and 0.582 +/- 0.051 M (circle dot) for the Ba (primary) and Bb (secondary) components, respectively. Spectral energy distribution (SED) modeling of the B subsystem suggests that the B circumstellar material is a source of extinction along the line of sight to the B components. This seems to corroborate a conjecture by Tokovinin that the B subsystem is viewed through circumbinary material, but it raises important questions about the morphology of that circumbinary material. Our modeling of the subsystem component SEDs finds temperatures and luminosities in agreement with previous studies, and coupled with the component mass estimates allows for comparison with PMS models in the low-mass regime with few empirical constraints. Solar abundance models seem to underpredict the inferred component temperatures and luminosities, while assuming slightly subsolar abundances brings the models and observations into better agreement. The current preliminary orbit does not yet place significant constraints on existing PMS stellar models, but prospects for additional observations improving the orbit model and component parameters are very good. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Lowell Observ, Flagstaff, AZ 86001 USA. RP Boden, AF (reprint author), CALTECH, Michelson Sci Ctr, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM bode@ipac.caltech.edu NR 32 TC 63 Z9 63 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 442 EP 451 DI 10.1086/497328 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600034 ER PT J AU De Buizer, JM Osorio, M Calvet, N AF De Buizer, JM Osorio, M Calvet, N TI Observations and modeling of the 2-25 mu m emission from high-mass protostellar object candidates SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : ISM; ISM : individual (G11.94-0.62, G29.96-0.02, G45.07+0.13); stars : early-type; stars : formation; stars : pre-main sequence ID H-II REGIONS; HOT MOLECULAR CORE; STAR-FORMING REGIONS; MIDINFRARED DETECTION; HII-REGIONS; G29.96-0.02; COMPACT; AMMONIA; ENVIRONMENTS; RESOLUTION AB This is a report on detailed modeling of young high-mass protostellar candidates during their most embedded and obscured phases. We performed narrowband mid-infrared imaging of three candidate high-mass protostellar objects in G11.94-0.62, G29.96-0.02, and G45.07+0.13 at Gemini Observatory using the Thermal-Region Camera and Spectrograph (T-ReCS). The sources were imaged through up to 11 narrowband filters, sampling their SEDs over the entire 2-25 mu m infrared range. For the first time, we have fit the observed SEDs of massive protostars with models that take into account departures from spherical symmetry in the infalling envelopes. In this way, we have been able to derive from the models the detailed physical parameters for these earliest stages of massive stellar life. Our detailed modeling suggests that massive star formation can proceed in a way very similar to the formation of low-mass stars. C1 Gemini Observat, La Serena, Chile. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP De Buizer, JM (reprint author), Gemini Observat, Casilla 603, La Serena, Chile. EM jdebuizer@gemini.edu; osorio@iaa.es; ncalvet@cfa.harvard.edu NR 47 TC 19 Z9 19 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 452 EP 465 DI 10.1086/497259 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600035 ER PT J AU Guenther, DB Kallinger, T Reegen, P Weiss, WW Matthews, JM Kuschnig, R Marchenko, S Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH AF Guenther, DB Kallinger, T Reegen, P Weiss, WW Matthews, JM Kuschnig, R Marchenko, S Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH TI Stellar model analysis of the oscillation spectrum of eta Bootis obtained from MOST SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (eta Bootis); stars : interiors; stars : oscillations ID STANDARD SOLAR MODEL; PHOTOMETRY; ASTEROSEISMOLOGY; FREQUENCIES; SEISMOLOGY; PULSATIONS; OPACITIES; SPACE AB Eight consecutive low-frequency radial p-modes are identified in the G0 IV star eta Bootis based on 27 days of ultraprecise rapid photometry obtained by the MOST (Microvariability and Oscillations of Stars) satellite. The MOST data extend smoothly, to lower overtones, the sequence of radial p-modes reported in earlier ground-based spectroscopy by other groups. The sampling is nearly continuous; hence, the ambiguities in p-mode identifications due to aliases, such as the cycle day(-1) alias found in ground observations, are not an issue. The lower overtone modes from the MOST data constrain the interior structure of the model of eta Boo, giving a best fit on a grid of similar to 300,000 stellar models for a composition of (X, Z) (0.71, 0.04), a mass of M 1.71 +/- 0.05 M-circle dot, and an age of t 2.40 +/- 0.03 Gyr. The surface temperature and luminosity of this model, which were constrained only by using the oscillation modes, are close (1 sigma) to current best estimates of eta Boo's surface temperature and luminosity. With the interior fit anchored by the lower overtone modes seen by MOST, standard models are not able to fit the higher overtone modes with the same level of accuracy. The discrepancy, model minus observed frequency, increases from 0.5 mu Hz at 250 mu Hz to 5 mu Hz at 1000 mu Hz and is similar to the discrepancy that exists between the Sun's observed p-mode frequencies and the p-mode frequencies of the standard solar model. This discrepancy promises to be a powerful constraint on models of three-dimensional convection. C1 St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. Univ British Columbia, Dept Phys & Astron, Vancouver, BC B6T 1Z1, Canada. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. Univ Toronto, David Dunlap Observat, Dept Phys & Astron, Montreal, PQ L4C 4Y6, Canada. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guenther, DB (reprint author), St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. NR 33 TC 20 Z9 20 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 547 EP 559 DI 10.1086/497387 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600046 ER PT J AU Gaudi, BS Bloom, JS AF Gaudi, BS Bloom, JS TI Astrometric microlensing constraints on a massive body in the outer solar system with GAIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; gravitational lensing; methods : data analysis; Oort Cloud ID COMET SHOWERS; OORT CLOUD; EXTINCTIONS; COMPANION; PLANET; GALAXY; STARS AB A body in solar orbit beyond the Kuiper Belt exhibits an annual parallax that exceeds its apparent proper motion by up to many orders of magnitude. Apparent motion of this body along the parallactic ellipse will deflect the angular position of background stars due to astrometric microlensing ("induced parallax''). By synoptically sampling the astrometric position of background stars over the entire sky, constraints on the existence ( and basic properties) of a massive nearby body may be inferred. With a simple simulation, we estimate the signal-to-noise ratio for detecting such a body-as a function of mass, heliocentric distance, and ecliptic latitude-using the anticipated sensitivity and temporal cadences from Gaia ( launch date 2011). A Jupiter-mass (M-J) object at 2000 AU is detectable by Gaia over the whole sky above 5 sigma, with even stronger constraints if it lies near the ecliptic plane. Hypotheses for the mass (similar to 3M(J)), distance (similar to 20,000 AU), and location of the proposed perturber ("Planet X''), which gives rise to long-period comets, may be testable. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Gaudi, BS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MC 20, Cambridge, MA 02138 USA. RI Gaudi, Bernard/I-7732-2012 NR 24 TC 15 Z9 15 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 DEC 10 PY 2005 VL 635 IS 1 BP 711 EP 717 DI 10.1086/497391 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600059 ER PT J AU Luhman, KL Adame, L D'Alessio, P Calvet, N Hartmann, L Megeath, ST Fazio, GG AF Luhman, KL Adame, L D'Alessio, P Calvet, N Hartmann, L Megeath, ST Fazio, GG TI Discovery of a planetary-mass brown dwarf with a circumstellar disk SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems : protoplanetary disks; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID SPITZER-SPACE-TELESCOPE; STAR-FORMING REGION; MAIN-SEQUENCE STARS; ACCRETION DISKS; YOUNG OBJECTS; SUBSTELLAR OBJECTS; INFRARED-SPECTRA; CHAMELEON-I; MODELS; TAURUS AB Using the Hubble Space Telescope, the 4 m Blanco Telescope at the Cerro Tololo Inter-American Observatory, and the Spitzer Space Telescope, we have performed deep imaging from 0.8 to 8 mu m of the southern subcluster in the Chamaeleon I star-forming region. In these data, we have discovered an object, Cha 110913-773444, whose colors and magnitudes are indicative of a very low mass brown dwarf with a circumstellar disk. In a near-infrared spectrum of this source obtained with the Gemini Near-Infrared Spectrograph, the presence of strong steam absorption confirms its late-type nature (greater than or similar to M9.5) while the shapes of the H- and K-band continua and the strengths of the Na I and K I lines demonstrate that it is a young, pre-main-sequence object rather than a field dwarf. A comparison of the bolometric luminosity of Cha 110913-773444 to the luminosities predicted by the evolutionary models of Chabrier & Baraffe and Burrows and coworkers indicates a mass of 8(-3)(+7)M(J), placing it fully within the mass range observed for extrasolar planetary companions (M less than or similar to 15M(J)). The spectral energy distribution of this object exhibits mid-infrared excess emission at lambda > 5 mu m, which we have successfully modeled in terms of an irradiated viscous accretion disk with M less than or similar to 10(-12) M(circle dot) yr(-1). Cha 110913-773444 is now the least massive brown dwarf observed to have a circumstellar disk, and indeed is one of the least massive free- floating objects found to date. These results demonstrate that the raw materials for planet formation exist around free-floating planetary-mass bodies. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. 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 Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM kluhman@astro.psu.edu; adamel@astroscu.unam.mx; p.dalessio@astrosmo.unam.mx; ncalve@umich.edut; lhartm@umich.edu; tmegeath@cfa.harvard.edu; gfazio@cfa.harvard.edu OI Adame, Lucia/0000-0002-6328-6099 NR 33 TC 63 Z9 63 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 DEC 10 PY 2005 VL 635 IS 1 BP L93 EP L96 DI 10.1086/498868 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700024 ER PT J AU Quataert, E Loeb, A AF Quataert, E Loeb, A TI Nonthermal Thz to TeV emission from stellar wind shocks in the galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : center; radiation mechanisms : nonthermal; radiation mechanisms : thermal ID SAGITTARIUS-A-ASTERISK; ENERGY GAMMA-RAYS; SUPERNOVA REMNANT; ACCRETION RATE; BLACK-HOLE; X-RAYS; ACCELERATION; GALAXY; POLARIZATION; DIRECTION AB The central parsec of the Galaxy contains dozens of massive stars with a cumulative mass-loss rate of similar to 10(-3) M-circle dot yr(-1). Shocks among these stellar winds produce the hot plasma that pervades the central part of the Galaxy. We argue that these stellar wind shocks also efficiently accelerate electrons and protons to relativistic energies. The relativistic electrons inverse Compton scatter the ambient ultraviolet and far-infrared radiation field, producing high-energy gamma-rays with a roughly constant luminosity from similar to GeV to similar to 10 TeV. This can account for the TeV source seen by HESS in the Galactic center. Our model predicts a GLAST counterpart to the HESS source with a luminosity of approximate to 10(35) ergs s(-1) and cooling break at approximate to 4 GeV. Synchrotron radiation from the same relativistic electrons should produce detectable emission at lower energies, with a surface brightness of approximate to 10-B-14(-3)2 ergs s(-1) cm(-2) arcsec(-2) from similar to THz to similar to keV, where B-3 is the magnetic field strength in units of mG. The observed level of diffuse thermal X-ray emission in the central parsec requires mG in our models. Future detection of B <= 300 the diffuse synchrotron background in the central parsec can directly constrain the magnetic field strength, providing an important boundary condition for models of accretion onto Sgr A*. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Quataert, E (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM eliot@astron.berkeley.edu; aloeb@cfa.harvard.edu NR 33 TC 17 Z9 17 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP L45 EP L48 DI 10.1086/499126 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700012 ER PT J AU Walker, GAH Kuschnig, R Matthews, JM Cameron, C Saio, H Lee, U Kambe, E Masuda, S Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Walker, GAH Kuschnig, R Matthews, JM Cameron, C Saio, H Lee, U Kambe, E Masuda, S Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW TI Most detects g-modes in the Be star HD 163868 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : early-type; stars : emission-line, Be; stars : individual (HD 163868); stars : oscillations; stars : rotation ID PULSATING B-STARS; MAIN-SEQUENCE STARS; NONRADIAL OSCILLATIONS; PHOTOMETRY; HIPPARCOS; STABILITY; SAMPLE; SPACE AB We have extracted a 37 day light curve with a precision of 0.0012 mag per point for the Microvariability and Oscillations of Stars (MOST) guide star, HD 163868 (B5 Ve). Its rich frequency spectrum resembles that of a slowly pulsating B (SPB) star but, being a rapid rotator, we designate it SPBe. The 60 most significant periods lie in three distinct groups centered on 8 days and 14 and 7 hr. We demonstrate that the 14 and 7 hr periods can be modeled by two swarms of high-order, prograde sectorial g-modes (m = -1 -2), which are destabilized by the iron opacity bump. Our model also predicts a group of r- modes with periods near 2.3 days, which correspond to frequencies observed in the tail of the 8 day group. The remaining periodicities, between 7 and 11 days, cannot be explained by unstable modes in our model. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Tohoku Univ, Grad Sch Sci, Inst Astron, Sendai, Miyagi 9808578, Japan. Natl Def Acad, Dept Earth & Ocean Sci, Yokosuka, Kanagawa 2398686, Japan. Natl Astron Observ, Okayama Astrophys Observ, Kamogata, Okayama 7190232, Japan. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Observ Mont Megant, Dept Phys, Montreal, PQ H3C 3J7, Canada. Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Walker, GAH (reprint author), 1234 Hewlett Pl, Victoria, BC V8S 4P7, Canada. EM gordonwa@uvic.ca; kuschnig@astro.phys.ubc.ca; matthews@phas.ubc.ca; ccameron@phas.ubc.ca; saio@astr.tohuku.ac.jp; lee@astr.tohuku.ac.jp; kambe@nda.ac.jp; masuda@oao.nao.ac.jp; guenther@ap.stmarys.ca; moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca; sasselov@cfa.harvard.edu; weiss@astro.univie.ac.at NR 25 TC 41 Z9 41 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP L77 EP L80 DI 10.1086/499362 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700020 ER PT J AU Weber, MA Schmelz, JT DeLuca, EE Roames, JK AF Weber, MA Schmelz, JT DeLuca, EE Roames, JK TI Isothermal bias of the "filter ratio" method for observations of multithermal plasma SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; Sun : corona; Sun : UV radiation ID TRANSITION-REGION; CORONAL-EXPLORER; ACTIVE-REGION; SOLAR CORONA; LOOPS; TEMPERATURE; TRACE; EIT; TELESCOPE AB An early result from the Transition Region and Coronal Explorer (TRACE) was that the EUV filter ratios for many narrow coronal loops (widths of a few arcseconds) were found to cluster within the small range 0.50-1.70, as functions of position along loop length. The most common interpretation is that the temperature along the loop is in fact nearly constant with a value between 1.1 and 1.3 MK. This interpretation has resulted in a class of TRACE loop models with heating close to the footpoints. We analyze the filter ratio method to show that the constant TRACE 195 angstrom/173 angstrom ratios can be reproduced by multithermal differential emission measures (DEMs) along the line of sight over a wide range of peak temperatures, so long as the distribution is relatively flat and spans the temperature response of both channels. Furthermore, in the limit of flat (i.e., very multithermal) DEMs, the filter ratio method is biased toward the ratio of the integrals of the temperature response functions. This result is general to any measurement of intensity ratios that are formed over a nonzero temperature range (e.g., narrow passbands and ion emission lines). C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Memphis, Dept Phys, Memphis, TN 38152 USA. RP Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mweber@cfa.harvard.edu; jschmelz@memphis.edu; deluca@cfa.harvard.edu; jroames@midsouth.rr.com RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 23 TC 35 Z9 35 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2005 VL 635 IS 1 BP L101 EP L104 DI 10.1086/499125 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700026 ER PT J AU Yu, ZH Higgins, KJ Klemperer, W McCarthy, MC Thaddeus, P AF Yu, ZH Higgins, KJ Klemperer, W McCarthy, MC Thaddeus, P TI Nuclear hyperfine interaction of rotating hydrogen: A spectroscopic investigation of hydrogen-OCS van der Waals complexes SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID DROPLETS; CLUSTERS AB The rotational spectra of five weakly bonded hydrogen-OCS complexes (paraH(2), orthoH(2), HD, orthoD(2), and paraD(2)) are measured. Hyperfine structure is resolved and analyzed in all except the complex with paraH(2), where I=0. For the two j=1 species, orthoH(2)-OCS and paraD(2)-OCS, nuclear hyperfine coupling constants are found to be d(a)=21.2(2) and 8.4(2) kHz, respectively, indicative of nearly free uniaxial rotation of the hydrogen around the b-inertial axis. Similar analyses for HD-OCS and orthoD(2)-OCS yield the quadrupole coupling constants eqQ(a)=16(2) and 30(2) kHz, respectively, showing that the internal rotational motions of HD and orthoD(2) in the complex are slightly hindered producing a small nonspherical distribution. For orthoD(2)-OCS, the observed hyperfine structure indicates that the nuclear spin states I=0 and 2 are strongly coupled in the rotation of the complex. (c) 2005 American Institute of Physics. C1 Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yu, ZH (reprint author), Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. NR 14 TC 14 Z9 14 U1 0 U2 5 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 DEC 8 PY 2005 VL 123 IS 22 AR 221106 DI 10.1063/1.2147306 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 995RF UT WOS:000234120800006 PM 16375463 ER PT J AU Wood, J AF Wood, J TI Alastair Cameron (1925-2005) - Astrophysicist and planetary scientist. Obituary SO NATURE LA English DT Biographical-Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wood, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jawood@alum.mit.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 752 EP 752 DI 10.1038/438752a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800029 PM 16341002 ER PT J AU Eisaman, MD Andre, A Massou, F Fleischhauer, M Zibrov, AS Lukin, MD AF Eisaman, MD Andre, A Massou, F Fleischhauer, M Zibrov, AS Lukin, MD TI Electromagnetically induced transparency with tunable single-photon pulses SO NATURE LA English DT Article ID QUANTUM COMMUNICATION; ATOMIC ENSEMBLES; LIGHT; GENERATION; STORAGE; OPTICS; MEMORY; PAIRS; GAS AB Techniques to facilitate controlled interactions between single photons and atoms are now being actively explored(1-7). These techniques are important for the practical realization of quantum networks, in which multiple memory nodes that utilize atoms for generation, storage and processing of quantum states are connected by single-photon transmission in optical fibres(1,2). One promising avenue for the realization of quantum networks involves the manipulation of quantum pulses of light in optically dense atomic ensembles using electromagnetically induced transparency (EIT, refs 8, 9). EIT is a coherent control technique that is widely used for controlling the propagation of classical, multi-photon light pulses(10-14) in applications such as efficient nonlinear optics(15). Here we demonstrate the use of EIT for the controllable generation, transmission and storage of single photons with tunable frequency, timing and bandwidth. We study the interaction of single photons produced in a 'source' ensemble of Rb-87 atoms at room temperature with another 'target' ensemble. This allows us to simultaneously probe the spectral and quantum statistical properties of narrow-bandwidth single-photon pulses, revealing that their quantum nature is preserved under EIT propagation and storage. We measure the time delay associated with the reduced group velocity of the single-photon pulses and report observations of their storage and retrieval. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tech Univ Kaiserslautern, Fachbereich Phys, D-67663 Kaiserslautern, Germany. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Eisaman, MD (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM eisaman@fas.harvard.edu RI Eisaman, Matthew/E-8006-2011; Fleischhauer, Michael/G-6716-2011; Zibrov, Alexander/G-7419-2014 OI Eisaman, Matthew/0000-0002-3814-6430; NR 30 TC 466 Z9 479 U1 4 U2 67 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 837 EP 841 DI 10.1038/nature04327 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800047 PM 16341010 ER PT J AU Hall, JPW AF Hall, JPW TI Montane speciation patterns in Ithomiola butterflies (Lepidoptera : Riodinidae): are they consistently moving up in the world? SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE biogeography; Ithomiola; montane; parapatric speciation; Riodinidae; vertical speciation ID ANDEAN BIRDS; LIMITS; DIVERSIFICATION; BIOGEOGRAPHY; NYMPHALIDAE; PHYLOGENIES; EXTINCTION; GRADIENTS; AMAZONIA; ECOLOGY AB Tropical lowland areas have often been seen as the centres of terrestrial species proliferation, but recent evidence suggests that young species may be more frequent in montane areas. Several montane speciation modes have been proposed, but their relative frequencies and predominant evolutionary sequence remain unclear because so few biogeographic and phylogenetic studies have tested such questions. I use morphological data to generate a phylogenetic hypothesis for all 11 species of the riodinid butterfly genus Ithomiola (Riodininae: Mesosemiini: Napaeina). These species are shown here to be all strictly geographically and elevationally allo- or parapatrically distributed with respect to their closest relatives in lowland and montane regions throughout the Neotropics. The overwhelming pattern in Ithomiola is of repeated upward parapatric speciation across an elevational gradient, and the genus appears to provide the clearest example to date of vertical montane speciation. All of the young derived species are montane and all of the old basal species are confined to the lowlands, supporting the hypothesis of montane regions largely as 'species pumps' and lowland regions as 'museums'. Possible reasons for the post-speciation maintenance of parapatric ranges in Ithomiola are discussed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM hallja@si.edu NR 50 TC 63 Z9 65 U1 1 U2 11 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 DEC 7 PY 2005 VL 272 IS 1580 BP 2457 EP 2466 DI 10.1098/rspb.2005.3254 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 990NY UT WOS:000233751700002 PM 16271969 ER PT J AU Whinnett, A Zimmermann, M Willmott, KR Herrera, N Mallarino, R Simpson, F Joron, M Lamas, G Mallet, J AF Whinnett, A Zimmermann, M Willmott, KR Herrera, N Mallarino, R Simpson, F Joron, M Lamas, G Mallet, J TI Strikingly variable divergence times inferred across an Amazonian butterfly 'suture zone' SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Lepidoptera; mitochondrial DNA; phylogeography; speciation; Pleistocene refuge hypothesis; DNA barcodes ID MITOCHONDRIAL-DNA; HELICONIUS BUTTERFLIES; MOLECULAR CLOCKS; EVOLUTION; LEPIDOPTERA; SPECIATION; DIVERSITY; PATTERNS; DIFFERENTIATION; BIOGEOGRAPHY AB 'Suture zones' are areas where hybrid and contact zones of multiple taxa are clustered. Such zones have been regarded as strong evidence for allopatric divergence by proponents of the Pleistocene forest refugia theory, a vicariance hypothesis frequently used to explain diversification in the Amazon basin. A central prediction of the refugia and other vicariance theories is that the taxa should have a common history so that divergence times should be coincident among taxa. A suture zone for Ithomiinae butterflies near Tarapoto, NE Peru, was therefore studied to examine divergence times of taxa in contact across the zone. We sequenced 161.9 bp of the mitochondrial COI/COII region in 172 individuals of 31 species from across the suture zone. Inferred divergence times differed remarkably, with divergence between some pairs of widespread species (each of which may have two or more subspecies interacting in the zone, as in the genus Melinaea) being considerably less than that between hybridizing subspecies in other genera (for instance in Oleria). Our data therefore strongly refute a simple hypothesis of simultaneous vicariance and suggest that ongoing parapatric or other modes of differentiation in continuous forest may be important in driving diversification in Amazonia. C1 UCL, Galton Lab, London NW1 2HE, England. Nat Hist Museum, London SW7 5BD, England. Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera, Gainesville, FL 32611 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Edinburgh, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. Univ Nacl Mayor San Marcos, Museo Hist Nat, Lima 14, Peru. RP Mallet, J (reprint author), UCL, Galton Lab, 4 Stephenson Way, London NW1 2HE, England. EM j.mallet@ucl.ac.uk RI Joron, Mathieu/C-9178-2009; mallet, james/B-5114-2008; OI Joron, Mathieu/0000-0003-1043-4147; Mallet, James/0000-0002-3370-0367; Lamas, Gerardo/0000-0002-3664-6730 NR 48 TC 49 Z9 52 U1 1 U2 17 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 DEC 7 PY 2005 VL 272 IS 1580 BP 2525 EP 2533 DI 10.1098/rspb.2005.3247 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 990NY UT WOS:000233751700012 PM 16271979 ER PT J AU Kirby, MX MacFadden, B AF Kirby, MX MacFadden, B TI Was southern Central America an archipelago or a peninsula in the middle miocene? A test using land-mammal body size SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Panama; land mammal; body size; miocene; paleobiogeography; cucaracha formation ID WESTERN PANAMA; ISLAND RULE; ISTHMUS; EVOLUTION; BRIDGE; VERTEBRATES; EXTINCTION; EMERGENCE; MOLLUSKS; ENDEMISM AB There has been considerable discussion about the complex geological history of southern Central America in the late Cenozoic prior to the closing of the Isthmus of Panama during the Pliocene. It is particularly unclear how far nuclear Central America extended southward as a continuous land connection with North America versus the alternate paleogeographic reconstruction of an extensive island-arc system during this time. In modem faunas, terrestrial mammal body sizes have fundamentally different patterns within regions of continuous land-mass versus island populations as a result of the "island rule." Variation in body size is relatively limited in species with continent-wide distributions, whereas, relative to mainland populations, those on islands can have as much as a four-fold increase, or decrease, in body size. Using tooth molar dimensions as a proxy for body mass, tooth size is compared from a middle Miocene land-mammal fauna from Panama (Gaillard Cut Local Fauna) relative to contemporaneous faunas in North America. Among six species, there is no significant difference in tooth size between Panama and North America. A second test comparing the artiodactyl Paratoceras wardi between Panama and Texas shows a significant difference in tooth size, with P wardi from Panama having slightly larger teeth (104% to 112% larger) than P wardi from Texas. This difference in size, however, is small compared to that predicted from insular evolution and is more consistent with the amount of variation seen in continent-wide species distributions. Results from both tests are consistent with the hypothesis that southern Central America had a dry-land connection to North America during the middle Miocene. Based on these data, there is no support for the alternate hypothesis of an extensive archipelago in southern Central America during this time. (c) 2005 Elsevier B.V. All rights reserved. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 2072, Balboa, Panama. EM kirbym@ancon.si.edu NR 50 TC 51 Z9 52 U1 1 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 5 PY 2005 VL 228 IS 3-4 BP 193 EP 202 DI 10.1016/j.palaeo.2005.06.002 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 989PB UT WOS:000233685000001 ER PT J AU Abatis, D Vagias, C Galanakis, D Norris, JN Moreau, D Roussakis, C Roussis, V AF Abatis, D Vagias, C Galanakis, D Norris, JN Moreau, D Roussakis, C Roussis, V TI Atomarianones A and B: two cytotoxic meroditerpenes from the brown alga Taonia atomaria SO TETRAHEDRON LETTERS LA English DT Article DE Taonia atomaria; meroditerpenes; atomarianones; cytotoxic; chemotaxonomy ID MARINE NATURAL PRODUCT; STYPOPODIUM-ZONALE; CHEMICAL-SHIFTS; NMR; SESQUITERPENES; HYDROQUINONES; FLABELLIFORME; SPECTROSCOPY; DICTYOTALES; METABOLITES AB Two novel cyclized meroditerpenoids atomarianones A, and B (I and 2), were isolated from the organic extract of the brown alga Taonia atomaria collected at Serifos island in the Central Aegean Sea. This is only the second report on metabolites having a functionalized indane moiety instead of a benzofurano- or a benzopyrano-ring connecting their aromatic and diterpenoid parts. Atomarianone A contains an unprecedented cis B-C ring fusion while atomarianone B is the epimer of A at C-7. Both metabolites were found to exhibit significant cytotoxic activity against two lung cancer cell lines. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Athens, Sch Pharm, Dept Pharmacognosy & Chem Nat Prod, GR-15771 Athens, Greece. Aristotle Univ Thessaloniki, Sch Pharm, Dept Pharmaceut Chem, Thessaloniki 54124, Greece. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. ISOMer, Lab Pharmacogenom Marine, Fac Pharm, F-44035 Nantes, France. RP Roussis, V (reprint author), Univ Athens, Sch Pharm, Dept Pharmacognosy & Chem Nat Prod, GR-15771 Athens, Greece. EM roussis@pharm.uoa.gr RI Moreau, Dimitri/E-5092-2012; Moreau, Dimitri/A-7503-2017 OI Moreau, Dimitri/0000-0002-9282-3324; Moreau, Dimitri/0000-0002-9282-3324 NR 34 TC 13 Z9 13 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4039 J9 TETRAHEDRON LETT JI Tetrahedron Lett. PD DEC 5 PY 2005 VL 46 IS 49 BP 8525 EP 8529 DI 10.1016/j.tetlet.2005.10.007 PG 5 WC Chemistry, Organic SC Chemistry GA 985KN UT WOS:000233376400016 ER PT J AU Irwin, RP Howard, AD Craddock, RA Moore, JM AF Irwin, RP Howard, AD Craddock, RA Moore, JM TI An intense terminal epoch of widespread fluvial activity on early Mars: 2. Increased runoff and paleolake development SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID MARGARITIFER SINUS; MARTIAN HIGHLANDS; VALLEY NETWORKS; GALE-CRATER; AQUEOUS SEDIMENTATION; DRAINAGE BASINS; FRETTED TERRAIN; IMPACT CRATERS; SUN PARADOX; YOUNG SUN AB [1] To explain the much higher denudation rates and valley network development on early Mars (> similar to 3.6 Gyr ago), most investigators have invoked either steady state warm/wet (Earthlike) or cold/dry ( modern Mars) end-member paleoclimates. Here we discuss evidence that highland gradation was prolonged, but generally slow and possibly ephemeral during the Noachian Period, and that the immature valley networks entrenched during a brief terminal epoch of more erosive fluvial activity in the late Noachian to early Hesperian. Observational support for this interpretation includes ( 1) late-stage breaching of some enclosed basins that had previously been extensively modified, but only by internal erosion and deposition; ( 2) deposition of pristine deltas and fans during a late stage of contributing valley entrenchment; ( 3) a brief, erosive response to base level decline ( which was imparted as fretted terrain developed by a suite of processes unrelated to surface runoff) in fluvial valleys that crosscut the highland-lowland boundary scarp; and ( 4) width/contributing area relationships of interior channels within valley networks, which record significant late-stage runoff production with no evidence of recovery to lower-flow conditions. This erosion appears to have ended abruptly, as depositional landforms generally were not entrenched with declining base level in crater lakes. A possible planetwide synchronicity and common cause to the late-stage fluvial activity are possible but remain uncertain. This increased activity of valley networks is offered as a possible explanation for diverse features of highland drainage basins, which were previously cited to support competing warm, wet and cold, dry paleoclimate scenarios. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20013 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, 6th St & Independence Ave SW, Washington, DC 20013 USA. EM irwinr@si.edu; ah6p@virginia.edu; jeff.moore@nasa.gov RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 114 TC 103 Z9 104 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 2 PY 2005 VL 110 IS E12 AR E12S15 DI 10.1029/2005JE002460 PG 38 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 993OM UT WOS:000233963400005 ER PT J AU Pfretzschner, HU Martin, T Maisch, MW Matzke, AT Sun, G AF Pfretzschner, HU Martin, T Maisch, MW Matzke, AT Sun, G TI A new docodont mammal from the Late Jurassic of the Junggar Basin in northwest China SO ACTA PALAEONTOLOGICA POLONICA LA English DT Article DE Docodonta; Dsungarodon; occlusion; Jurassic; Qigu Formation; Junggar Basin ID MOLAR OCCLUSION; ENGLAND; MIDDLE AB Fieldwork in the early Late Jurassic (Oxfordian) Qigu Formation of the Junggar Basin in Northwest China (Xinjiang Autonomous Region) produced teeth and mandibular fragments of a new docodont. The new taxon has a large "pseudotalonid" on the lower molars, and by retention of crest b-g exhibits closer affinities to Simpsonodon and Krusatodon from the Middle Jurassic of Europe than to the other known Asian docodonts Tashkumyrodon,Tegotherium, and Sibirotherium. It differs from the Haldanodon-Docodon-lineage by the "pseudotalonid" and large cusps b and g. A PAUP analysis based on lower molar characters produced a single most parsimonious tree with two main clades. One clade comprises Docodon, Haldanodon, and Borealestes, and the other Dsungarodon, Simpsonodon, and Krusatodon plus the Asian tegotherrids. Analysis of the molar occlusal relationships using epoxy casts mounted on a micromanipulator revealed a four-phase chewing cycle with transverse component. The molars of the new docodont exhibit a well developed grinding function besides cutting and shearing, probably indicating an omnivorous or even herbivorous diet. A grinding and crushing function is also present in the molars of Simpsonodon, Krusatodon, and the Asian tegotheriids, whereas Borealestes, Haldanodon, and Docodon retain the plesiomorphic molar pattern with mainly piercing and cutting function. C1 Univ Tubingen, Inst Geowissensch, D-72076 Tubingen, Germany. Forsch Inst Senckenberg, D-60325 Frankfurt, Germany. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. Jilin Univ, Res Ctr Paleontol, Changchun 130026, Peoples R China. RP Pfretzschner, HU (reprint author), Univ Tubingen, Inst Geowissensch, Sigwartstr 10, D-72076 Tubingen, Germany. EM hans-ulrich.pfretzschner@unt-tuebingen.de; tmartin@senckenberg.de; michael.maisch@unt-tuebingen.de; matzkea@si.edu; sunge@jlu.edu.cn NR 33 TC 14 Z9 26 U1 1 U2 2 PU INSTYTUT PALEOBIOLOGII PAN PI WARSAW PA UL TWARDA 51/55, 00-818 WARSAW, POLAND SN 0567-7920 J9 ACTA PALAEONTOL POL JI Acta Palaeontol. Pol. PD DEC PY 2005 VL 50 IS 4 BP 799 EP 808 PG 10 WC Paleontology SC Paleontology GA 991QS UT WOS:000233829300012 ER PT J AU Wesley-Hunt, GD Werdelin, L AF Wesley-Hunt, GD Werdelin, L TI Basicranial morphology and phylogenetic position of the upper Eocene carnivoramorphan Quercygale SO ACTA PALAEONTOLOGICA POLONICA LA English DT Article DE Mammalia; Miacidae; miacoidea; Quercygale; carnivoran phylogeny; basicranium; Eocene; Quercy ID AUDITORY BULLA; SYSTEMATICS; REVISION AB Quercygale angustidens is a small, early carnivoramorphan from the upper Eocene of northwest Europe including the Phosphorites du Quercy, France. Although there is extensive material of the genus, very little has been published on the auditory region which is an important character complex for taxonomy and phylogenetic studies. This paper presents a detailed description of the basicranium of an undistorted partial skull of Quercygale. The new data form the basis for a phylogenetic analysis of Quercygale in the context of basal carinvoramorphan interrelationships. Quercygale has a mix of derived and plesiomorphic characters. The promontorium is highly derived, and unlike that of any other "miacoid". Yet, based on the evidence from surrounding bones the bulla does not appear to be as expanded as in other closely related miacids. In the phylogenetic analysis Quercygale is the sister-taxon to Nimravidae and crown-group Carnivora, and it appears to be the most derived of the stem-group Miacidae. We discuss the implications that the position of Quercygale has on carnivoramorphan phylogenetics. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Swedish Museum Nat Hist, Dept Palaeozool, S-10405 Stockholm, Sweden. RP Wesley-Hunt, GD (reprint author), Smithsonian Inst, Dept Paleobiol, MRC NHB 121, Washington, DC 20560 USA. EM gina.wesley@nrm.sel; werdelin@nrm.se NR 50 TC 14 Z9 14 U1 0 U2 4 PU INST PALEOBIOLOGII PAN PI WARSAW PA UL TWARDA 51/55, 00-818 WARSAW, POLAND SN 0567-7920 EI 1732-2421 J9 ACTA PALAEONTOL POL JI Acta Palaeontol. Pol. PD DEC PY 2005 VL 50 IS 4 BP 837 EP 846 PG 10 WC Paleontology SC Paleontology GA 991QS UT WOS:000233829300015 ER PT J AU Laack, LL Tewes, ME Haines, AM Rappole, JH AF Laack, LL Tewes, ME Haines, AM Rappole, JH TI Reproductive life history of ocelots Leopardus pardalis in southern Texas SO ACTA THERIOLOGICA LA English DT Article DE Leopardus pardalis; den sites; fecundity; ocelot; reproduction; southern Texas ID EARLY MATERNAL-BEHAVIOR; SURVIVAL; MORTALITY; BOBCATS; RATES AB The ocelot Leopardus pardalis Linnaeus, 1758 is an endangered felid in the United States currently restricted to southern Texas. The objectives of our study were to obtain data on ocelot parturition dates, fecundity, sex ratios, den characteristics, and first year survival, all of which are critical in development of population viability models. Sixteen parturition events were recorded ranging from mid-April to late December for 12 wild ocelots. Cumulatively, litters consisted of 1 or 2 kittens ((x) over bar = 1.2 +/- 0.44 SD). Cumulative sex ratio was 1:2.5 (male:female); however, there was no significant difference between the observed sex ratio and a 1: 1 sex ratio. Ten den sites were in close proximity (<= 10 m) to dense thornshrub. Adult female ocelots used 2 to 4 den sites for each litter with distance between consecutively occupied dens ranging from 110 to 280 m ((x) over bar = 158 m +/- 93 SD). An estimated annual survival for ocelots 0 to 1 year of age was 0.68. Evidence suggests that ocelots in the wild may breed more frequently than had been previously hypothesized. C1 Laguna Atascosa Natl Wildlife Refuge, Los Fresnos, TX 78566 USA. Texas A&M Univ, Caesar Kleberg Wildlife Res Inst, Feline Res Program, Kingsville, TX 78363 USA. Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Laack, LL (reprint author), Laguna Atascosa Natl Wildlife Refuge, 22817 Ocelot Rd, Los Fresnos, TX 78566 USA. EM Linda_Laack@fws.gov NR 47 TC 10 Z9 10 U1 9 U2 25 PU POLISH ACAD SCIENCES PI BIALOWIEZA PA MAMMAL RESEARCH INST, 17-230 BIALOWIEZA, POLAND SN 0001-7051 J9 ACTA THERIOL JI Acta Theriol. PD DEC PY 2005 VL 50 IS 4 BP 505 EP 514 DI 10.1007/BF03192643 PG 10 WC Zoology SC Zoology GA 990ZL UT WOS:000233781800007 ER PT J AU Wong, SJ Dupuis, AP Kilpatrick, AM Marra, PP Glaser, AL Victor, T Daszak, P Kramer, LD AF Wong, Susan J. Dupuis, A. P., II Kilpatrick, A. M. Marra, P. P. Glaser, A. L. Victor, T. Daszak, P. Kramer, L. D. TI Comparison of indirect ELISA and plaque reduction neutralization to multiplex microsphere immunoassay for detection of antibodies to West Nile virus in blood of wild birds SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Meeting Abstract C1 [Wong, Susan J.; Dupuis, A. P., II; Victor, T.; Kramer, L. D.] NYSDOH, Wadsworth Ctr, Albany, NY USA. [Kilpatrick, A. M.; Daszak, P.] Consortium Conservat Med, New York, NY USA. [Marra, P. P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Glaser, A. L.] Cornell Univ, New York State Coll Vet Med, Ithaca, NY USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD DEC PY 2005 VL 73 IS 6 SU S MA 277 BP 92 EP 92 PG 1 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA V44GA UT WOS:000202990000277 ER PT J AU Kilpatrick, AM Jones, M Kramer, LD Marra, PP Daszak, P AF Kilpatrick, A. Marm Jones, Matthew Kramer, Laura D. Marra, Peter P. Daszak, Peter TI West Nile Virus vector ecology across an urbanization gradient SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Meeting Abstract C1 [Kilpatrick, A. Marm; Daszak, Peter] Consortium Conservat Med, New York, NY USA. [Jones, Matthew; Kramer, Laura D.] New York State Dept Hlth, Wadsworth Ctr, Albany, NY USA. [Marra, Peter P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. NR 0 TC 0 Z9 0 U1 0 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 DEC PY 2005 VL 73 IS 6 SU S MA 938 BP 307 EP 308 PG 2 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA V44GA UT WOS:000202990001361 ER PT J AU Brandao, RA Heyer, WR AF Brandao, RA Heyer, WR TI The complex calls of Leptodactylus pustulatus (Amphibia, Anura, Leptodactylidae) SO AMPHIBIA-REPTILIA LA English DT Article ID FROG C1 Inst Brasileiro Meio Ambiente, Diretoria Ecossitemas, BR-70818900 Brasilia, DF, Brazil. Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Brandao, RA (reprint author), Inst Brasileiro Meio Ambiente, Diretoria Ecossitemas, BR-70818900 Brasilia, DF, Brazil. EM reuberbrandao@yahoo.com.br; heyerr@si.edu RI Brandao, Reuber/A-3427-2013 OI Brandao, Reuber/0000-0003-3940-2544 NR 19 TC 3 Z9 5 U1 0 U2 0 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0173-5373 J9 AMPHIBIA-REPTILIA JI Amphib. Reptil. PD DEC PY 2005 VL 26 IS 4 BP 566 EP 570 DI 10.1163/156853805774806278 PG 5 WC Zoology SC Zoology GA 994WQ UT WOS:000234062300020 ER PT J AU Rogers, JD Ulambayar, E Gallon, M AF Rogers, JD Ulambayar, E Gallon, M TI Urban centres and the emergence of empires in Eastern Inner Asia SO ANTIQUITY LA English DT Article DE Mongolia; Mongol; civilisation; empire; urbanism AB The inner mechanics of Mongol empires are revealed through recent surveys by an American-Mongolian team. The large political confederations of high mobility which traditionally characterise the great Mongol empires of the first and second millennia AD are shown to have made use of highly sophisticated urban places which feature advanced planning and design, and impressive monumentality serving a variety of specific functions. Planning in eluded open spaces within the walls reserved for the erection of tents. C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Inst Archaeol, Ulaanbaatar, Mongol Peo Rep. Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. RP Rogers, JD (reprint author), Smithsonian Inst, Dept Anthropol, NHB 112, Washington, DC 20560 USA. EM rogers.daniel@nmnh.si.edu NR 66 TC 15 Z9 15 U1 0 U2 1 PU ANTIQUITY PI YORK PA KINGS MANOR, YORK YO1 7EP, ENGLAND SN 0003-598X J9 ANTIQUITY JI Antiquity PD DEC PY 2005 VL 79 IS 306 BP 801 EP 818 PG 18 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 996LM UT WOS:000234175400005 ER PT J AU Beaty, DW Clifford, SM Borg, LE Catling, DC Craddock, RA Des Marais, DJ Farmer, JD Frey, HV Haberle, RM McKay, CP Newsom, HE Parker, TJ Segura, T Tanaka, KL AF Beaty, DW Clifford, SM Borg, LE Catling, DC Craddock, RA Des Marais, DJ Farmer, JD Frey, HV Haberle, RM McKay, CP Newsom, HE Parker, TJ Segura, T Tanaka, KL TI Key science questions from the second conference on early Mars: Geologic, hydrologic, and climatic evolution and the implications for life SO ASTROBIOLOGY LA English DT Review DE early Mars; noachian; volatiles; habitability; water; geologic evolution ID MARTIAN IMPACT CRATERS; CARBON-DIOXIDE CLOUDS; HYDROTHERMAL ALTERATION; EARLY DIFFERENTIATION; TERRESTRIAL PLANETS; METEORITE ALH84001; FLUVIAL PROCESSES; GREENHOUSE GASES; ANCIENT OCEANS; LATE MAGMATISM AB In October 2004, more than 130 terrestrial and planetary scientists met in Jackson Hole, WY, to discuss early Mars. The first billion years of martian geologic history is of particular interest because it is a period during which the planet was most active, after which a less dynamic period ensued that extends to the present day. The early activity left a fascinating geological record, which we are only beginning to unravel through direct observation and modeling. In considering this time period, questions outnumber answers, and one of the purposes of the meeting was to gather some of the best experts in the field to consider the current state of knowledge, ascertain which questions remain to be addressed, and identify the most promising approaches to addressing those questions. The purpose of this report is to document that discussion. Throughout the planet's first billion years, planetary-scale processes-including differentiation, hydrodynamic escape, volcanism, large impacts, erosion, and sedimentation-rapidly modified the atmosphere and crust. How did these processes operate, and what were their rates and interdependencies? The early environment was also characterized by both abundant liquid water and plentiful sources of energy, two of the most important conditions considered necessary for the origin of life. Where and when did the most habitable environments occur? Did life actually occupy them, and if so, has life persisted on Mars to the present? Our understanding of early Mars is critical to understanding how the planet we see today came to be. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Mars Program Off, Pasadena, CA 91109 USA. Ames Res Ctr, Moffett Field, CA USA. Northrop Grumman, Redondo Beach, CA USA. Lunar & Planetary Inst, Houston, TX 77058 USA. Univ New Mexico, Albuquerque, NM 87131 USA. Univ Bristol, Dept Earth Sci, Bristol, Avon, England. Univ Washington, Seattle, WA 98195 USA. Smithsonian Inst, Washington, DC 20560 USA. Arizona State Univ, Tucson, AZ USA. Goddard Space Flight Ctr, Greenbelt, MD USA. US Geol Survey, Reston, VA 22092 USA. RP Beaty, DW (reprint author), CALTECH, Jet Prop Lab, Mail Stop 301-345,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Beaty@jpl.nasa.gov RI Catling, David/D-2082-2009; OI Catling, David/0000-0001-5646-120X NR 159 TC 12 Z9 14 U1 1 U2 14 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2005 VL 5 IS 6 BP 663 EP 689 DI 10.1089/ast.2005.5.663 PG 27 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 998WY UT WOS:000234351800001 PM 16379524 ER PT J AU Krisciunas, K Garnavich, PM Challis, P Prieto, JL Riess, AG Barris, B Aguilera, C Becker, AC Blondin, S Chornock, R Clocchiatti, A Covarrubias, R Filippenko, AV Foley, RJ Hicken, M Jha, S Kirshner, RP Leibundgut, B Li, WD Matheson, T Miceli, A Miknaitis, G Rest, A Salvo, ME Schmidt, BP Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB Tonry, JL Wood-Vasey, WM AF Krisciunas, K Garnavich, PM Challis, P Prieto, JL Riess, AG Barris, B Aguilera, C Becker, AC Blondin, S Chornock, R Clocchiatti, A Covarrubias, R Filippenko, AV Foley, RJ Hicken, M Jha, S Kirshner, RP Leibundgut, B Li, WD Matheson, T Miceli, A Miknaitis, G Rest, A Salvo, ME Schmidt, BP Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB Tonry, JL Wood-Vasey, WM TI Hubble Space Telescope observations of nine high-redshift essence supernovae SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : distances and redshifts; supernovae : general ID IA SUPERNOVAE; COSMOLOGICAL CONSTANT; HOST GALAXIES; LIGHT CURVES; DARK ENERGY; ACCELERATING UNIVERSE; PRECISE DISTANCE; BLACK-HOLE; SN 1991T; DIAGRAM AB We present broadband light curves of nine supernovae ranging in redshift from 0.5 to 0.8. The supernovae were discovered as part of the ESSENCE project, and the light curves are a combination of Cerro Tololo 4 m and Hubble Space Telescope (HST) photometry. On the basis of spectra and/or light-curve fitting, eight of these objects are definitely Type Ia supernovae, while the classification of one is problematic. The ESSENCE project is a 5 yr endeavor to discover about 200 high-redshift Type Ia supernovae, with the goal of tightly constraining the time average of the equation-of-state parameter [w = p/(rho c(2))] of the "dark energy." To help minimize our systematic errors, all of our ground-based photometry is obtained with the same telescope and instrument. In 2003 the highest redshift subset of ESSENCE supernovae was selected for detailed study with HST. Here we present the first photometric results of the survey. We find that all but one of the ESSENCE supernovae have slowly declining light curves and that the sample is not representative of the low-redshift set of ESSENCE Type Ia supernovae. This is unlikely to be a sign of evolution in the population. We attribute the decline-rate distribution of HST events to a selection bias at the high-redshift edge of our sample and find that such a bias will infect other magnitude-limited Type Ia supernova searches unless appropriate precautions are taken. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Cerro Tololo Interamer Observ, La Serena, Chile. Univ Washington, Dept Astron, Seattle, WA 98195 USA. European So Observ, D-85748 Garching, Germany. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Washington, Dept Phys, Seattle, WA 98195 USA. Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. AlbaNova, Stockholm Observ, SE-10691 Stockholm, Sweden. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. RP Krisciunas, K (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM kkrisciu@nd.edu; pgarnavi@nd.edu; pchallis@cfa.harvard.edu; prieto@astronomyohio-state.edu; ariess@stsci.edu; barris@ifa.hawaii.edu; caguilera@ctio.noao.edu; becker@astro.washington.edu; sblondin@eso.org; chornock@astro.berkeley.edu; aclocchi@astro.puc.cl; ricardo@astro.washington.edu; alex@astro.berkeley.edu; rfoley@astro.berkeley.edu; mhicken@cfa.harvard.edu; sjha@astro.berkeley.edu; kirshner@cfa.harvard.edu; bleibund@eso.org; weidong@astro.berkeley.edu; matheson@noao.edu; amiceli@astro.washington.edu; gm@u.washington.edu; arest@noao.edu; salvo@mso.anu.edu.au; brian@mso.anu.edu.au; csmith@noao.edu; jesper@astro.su.se; jspyromi@eso.org; cstubbs@fas.harvard.edu; nsuntzeff@noao.edu; jt@ifa.hawaii.edu; wmwood-vasey@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0001-6589-1287 NR 72 TC 34 Z9 34 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 DEC PY 2005 VL 130 IS 6 BP 2453 EP 2472 DI 10.1086/497640 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800002 ER PT J AU Giovanelli, R Haynes, MP Kent, BR Perillat, P Saintonge, A Brosch, N Catinella, B Hoffman, GL Stierwalt, S Spekkens, K Lerner, MS Masters, KL Momjian, E Rosenberg, JL Springob, CM Boselli, A Charmandaris, V Darling, JK Davies, J Lambas, DG Gavazzi, G Giovanardi, C Hardy, E Hunt, LK Iovino, A Karachentsev, ID Karachentseva, VE Koopmann, RA Marinoni, C Minchin, R Muller, E Putman, M Pantoja, C Salzer, JJ Scodeggio, M Skillman, E Solanes, JM Valotto, C van Driel, W van Zee, L AF Giovanelli, R Haynes, MP Kent, BR Perillat, P Saintonge, A Brosch, N Catinella, B Hoffman, GL Stierwalt, S Spekkens, K Lerner, MS Masters, KL Momjian, E Rosenberg, JL Springob, CM Boselli, A Charmandaris, V Darling, JK Davies, J Lambas, DG Gavazzi, G Giovanardi, C Hardy, E Hunt, LK Iovino, A Karachentsev, ID Karachentseva, VE Koopmann, RA Marinoni, C Minchin, R Muller, E Putman, M Pantoja, C Salzer, JJ Scodeggio, M Skillman, E Solanes, JM Valotto, C van Driel, W van Zee, L TI The Arecibo Legacy Fast ALFA survey. I. Science goals, survey design, and strategy SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; galaxies : halos; galaxies : luminosity function, mass function; galaxies : photometry; galaxies : spiral; radio lines : galaxies; surveys ID 21 CENTIMETER LINE; DUAL-BEAM SURVEY; HI MASS FUNCTION; ALL-SKY-SURVEY; VIRGO CLUSTER; IRREGULAR GALAXIES; NEUTRAL HYDROGEN; DWARF GALAXIES; HIPASS CATALOG; CLOUDS AB The recently initiated Arecibo Legacy Fast ALFA ( ALFALFA) survey aims to map similar to 7000 deg(2) of the high Galactic latitude sky visible from Arecibo, providing a H I line spectral database covering the redshift range between -1600 and 18,000 km s(-1) with similar to 5 km s(-1) resolution. Exploiting Arecibo's large collecting area and small beam size, ALFALFA is specifically designed to probe the faint end of the H I mass function in the local universe and will provide a census of H I in the surveyed sky area to faint flux limits, making it especially useful in synergy with wide-area surveys conducted at other wavelengths. ALFALFA will also provide the basis for studies of the dynamics of galaxies within the Local Supercluster and nearby superclusters, allow measurement of the H I diameter function, and enable a first wide-area blind search for local H I tidal features, H I absorbers at z < 0.06, and OH megamasers in the redshift range 0.16 < z < 0.25. Although completion of the survey will require some 5 years, public access to the ALFALFA data and data products will be provided in a timely manner, thus allowing its application for studies beyond those targeted by the ALFALFA collaboration. ALFALFA adopts a two-pass, minimum intrusion, drift scan observing technique that samples the same region of sky at two separate epochs to aid in the discrimination of cosmic signals from noise and terrestrial interference. Survey simulations, which take into account large-scale structure in the mass distribution and incorporate experience with the ALFA system gained from tests conducted during its commissioning phase, suggest that ALFALFA will detect on the order of 20,000 extragalactic H I line sources out to z similar to 0.06, including several hundred with H I masses M-HI < 10(7.5) M-circle dot. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Lafayette Coll, Hugel Sci Ctr, Easton, PA 18042 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Traverse Siphon, Astrophys Lab, F-13376 Marseille, France. Univ Crete, Dept Phys, Iraklion 71003, Greece. Carnegie Observ, Pasadena, CA 91101 USA. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina. Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Natl Radio Astron Observ, Santiago, Chile. INAF, Ist Radioastron, Sez Firenze, I-50125 Florence, Italy. Osserv Astron Brera, INAF, I-20121 Milan, Italy. Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia. Natl Taras Shevchenko Univ Kiev, Dept Astron & Space Sci, UA-252017 Kiev, Ukraine. Union Coll, Dept Phys & Astron, Schenectady, NY 12308 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA. Wesleyan Univ, Dept Astron, Middletown, CT 06457 USA. Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. CSIC, Inst Ciencias Espacio, Ctr Especial Recerca Astrofis Fis Particles & Cos, Madrid, Spain. Observ Meudon, F-92195 Meudon, France. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Giovanelli, R (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM riccardo@astro.cornell.edu; haynes@astro.cornell.edu; bkent@astro.cornell.edu; phil@naic.edu; amelie@astro.cornelledu; noah@wise.tau.ac.il; bcatinel@naic.edu; hoffmang@lafayette.edu; sabrina@astro.cornell.edu; spekkens@astro.cornell.edu; lerner@naic.edu; masters@astro.cornell.edu; emomjian@naic.edu; jlrosenberg@cfa.harvard.edu; springob@astro.cornell.edu; alessandro.boselli@oamp.fr; vassilis@physics.uoc.gr; darling@ociw.edu; jonathan.davies@astro.cf.ac.uk; dgl@oac.uncor.edu; giuseppe.gavazzi@mib.infn.it; giova@arcetri.astro.it; ehardy@nrao.edu; hunt@arcetri.astro.it; iovino@brera.mi.astro.it; ikar@sao.ru; vkarach@observ.univ.kiev.ua; koopmanr@union.edu; marinoni@brera.mi.astro.it; robert.minchin@astro.cf.acuk; erik.muller@atnf.csiro.au; mputman@umich.edu; cpantoja@naic.edu; slaz@astro.wesleyan.edu; marcos@mi.iasf.cnr.it; skillman@astro.umn.edu; jm.solanes@ub.edu; val@oac.uncor.edu; wim.vandriel@obspm.fr; vanzee@astro.indiana.edu RI Charmandaris, Vassilis/A-7196-2008; Darling, Jeremy/A-7968-2009; Brosch, Noah/C-7889-2009; Minchin, Robert/F-6343-2012; OI Charmandaris, Vassilis/0000-0002-2688-1956; Darling, Jeremy/0000-0003-2511-2060; Minchin, Robert/0000-0002-1261-6641; Iovino, Angela/0000-0001-6958-0304; Scodeggio, Marco/0000-0002-2282-5850; Catinella, Barbara/0000-0002-7625-562X; Hunt, Leslie/0000-0001-9162-2371; Masters, Karen/0000-0003-0846-9578 NR 36 TC 347 Z9 353 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2005 VL 130 IS 6 BP 2598 EP 2612 DI 10.1086/497431 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800013 ER PT J AU Giovanelli, R Haynes, MP Kent, BR Perillat, P Catinella, B Hoffman, GL Momjian, E Rosenberg, JL Saintonge, A Spekkens, K Stierwalt, S Brosch, N Masters, KL Springob, CM Karachentsev, ID Karachentseva, VE Koopmann, RA Muller, E van Driel, W van Zee, L AF Giovanelli, R Haynes, MP Kent, BR Perillat, P Catinella, B Hoffman, GL Momjian, E Rosenberg, JL Saintonge, A Spekkens, K Stierwalt, S Brosch, N Masters, KL Springob, CM Karachentsev, ID Karachentseva, VE Koopmann, RA Muller, E van Driel, W van Zee, L TI The Arecibo Legacy Fast ALFA survey. II. Results of precursor observations SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; galaxies : halos; galaxies : luminosity function, mass function; galaxies : photometry; galaxies : spiral; radio lines : galaxies ID 21 CENTIMETER LINE; ALL-SKY-SURVEY; HIPASS CATALOG; GALAXIES AB In preparation for the full Arecibo Legacy Fast ALFA (ALFALFA) extragalactic H I survey, precursor observations were carried out in 2004 August-September with the seven-beam Arecibo L-band Feed Array (ALFA) receiver system and the Wideband Arecibo Pulsar Processor spectral processors. While these observations were geared mainly at testing and debugging survey strategy, hardware, and software, approximately 48 hr of telescope time yielded science-quality data. The efficiency of system usage (allowing for minor malfunctions and the impact of radio-frequency interference) during that time was 75%. From those observations, an initial list of 730 tentative detections of varying degrees of reliability was extracted. Ninety-eight high signal-to-noise ratio candidates were deemed to be bona fide H I line detections. To test our ability to discriminate cosmic signals from radio-frequency interference and noise, 165 candidates ranging in reliability likelihood were reobserved with the single-beam L-band wide system at Arecibo in 2005 January-February. Of those, 41% were confirmed as real. We present the results of both the ALFA and the single-beam observations for the sample of 166 confirmed H I sources, as well as our assessment of their optical counterparts. Of the 166 sources, 62 coincided with previously known H I sources, while optical redshifts were available for an additional 18 galaxies; thus, 52% of the redshifts reported here were previously unknown. Of the 166 H I detections, 115 are identified with previously cataloged galaxies of either known or unknown redshift, leaving 51 objects identified for the first time. Because of the higher sensitivity of the Arecibo system, fewer than 10% of the 166 H I sources would have been detected by a HIPASS-like survey of the same region. Three of the objects have H I masses less than 107 M-circle dot. The full ALFALFA survey, which commenced in 2005 February, should detect more than 100 times as many objects of similarly low H I mass over the next 5 years. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. Lafayette Coll, Hugel Sci Ctr, Easton, PA 18042 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia. Kiev TG Shevchenko State Univ, Dept Astron & Space Sci, UA-252017 Kiev, Ukraine. Union Coll, Dept Phys & Astron, Schenectady, NY 12308 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Observ Meudon, F-92195 Meudon, France. Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Giovanelli, R (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM riccardo@astro.cornell.edu; haynes@astro.cornell.edu; bkent@astro.cornell.edu; phil@naic.edu; bcatinel@naic.edu; hoffmang@lafayette.edu; emomjian@naic.edu; jlrosenberg@cfa.harvard.edu; amelie@astro.cornell.edu; spekkens@astro.cornell.edu; sabrina@astro.cornell.edu; noah@wise.tau.ac.il; masters@astro.cornell.edu; springob@astro.cornell.edu; ikar@sao.ru; vkarach@observ.univ.kiev.ua; koopmanr@union.edu; erik.muller@atnf.csiro.au; wim.vandriel@obspm.fr; vanzee@astro.indiana.edu RI Brosch, Noah/C-7889-2009; OI Catinella, Barbara/0000-0002-7625-562X; Masters, Karen/0000-0003-0846-9578 NR 13 TC 60 Z9 60 U1 1 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 DEC PY 2005 VL 130 IS 6 BP 2613 EP 2624 DI 10.1086/497432 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800014 ER PT J AU Magnani, L Lugo, S Dame, TM AF Magnani, L Lugo, S Dame, TM TI CH 3 GHz observations of molecular clouds along the Galactic plane SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : molecules; radio lines : ISM; surveys ID DENSE INTERSTELLAR CLOUDS; H-2 CONVERSION FACTOR; TRANSLUCENT CLOUDS; RADIO OBSERVATIONS; MILKY-WAY; CO SURVEY; DIFFUSE; LATITUDES; CHEMISTRY; EMISSION AB Spectra in the CH (2)Pi(1/2), J = 1/2, F = 1-1 transition at 3335 MHz were obtained in three five-point crosses centered on the Galactic plane at l = 50 degrees, 100 degrees, and 110 degrees. The lines of sight traversed both giant molecular clouds (GMCs) and local, smaller entities. This transition is a good tracer of low-density molecular gas, and the line profiles are very similar to CO(1-0) data at nearly the same resolution. In addition, the CH 3335 MHz line can be used to calibrate the CO-H-2 conversion factor (X-CO) in low-density molecular gas. Although this technique underestimates X-CO in GMCs, our results are within a factor of 2 of X-CO values calibrated for GMCs by other techniques. The similarity of CH and CO line profiles, and that of X-CO values derived from CH and more traditional techniques, implies that most of the molecular gas along the observed lines of sight is at relatively low densities (n <= 10(3) cm(-3)). C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Magnani, L (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM loris@physast.uga.edu NR 29 TC 7 Z9 7 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 DEC PY 2005 VL 130 IS 6 BP 2725 EP 2731 DI 10.1086/497538 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800021 ER PT J AU Lacy, CHS Torres, G Claret, A Vaz, LPR AF Lacy, CHS Torres, G Claret, A Vaz, LPR TI Absolute properties of the eclipsing binary star RW Lacertae SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : evolution; stars : fundamental parameters; stars : individual (RW Lacertae) ID LIMB-DARKENING COEFFICIENTS; MAIN-SEQUENCE; LIGHT CURVES; SPECTROSCOPIC BINARIES; SYNCHRONIZATION TIMES; EVOLUTIONARY MODELS; Y-2 ISOCHRONES; PHOTOMETRY; CIRCULARIZATION; DIMENSIONS AB We present 3004 differential observations in the V bandpass measured by a robotic telescope, as well as 36 pairs of radial velocities from high-resolution spectroscopic observations, of the detached, eccentric, EA-type, 10.37 day period, double-lined eclipsing binary star RW Lac. Absolute dimensions of the components are determined with excellent precision ( better than 0.7% in the masses and 0.5% in the radii) for the purpose of testing various aspects of theoretical modeling. We obtain 0.928 +/- 0.006 M. and 1.186 +/- 0.004 R. for the hotter, larger, more massive, and more luminous photometric primary (star A) and 0.870 +/- 0.004 M. and 0.964 +/- 0.004 R. for the cooler, smaller, less massive, and less luminous photometric secondary (star B). A faint, third component contributes 2.6% of the light in V but is not detected in our spectrograms. The effective temperatures and interstellar reddening of the stars are accurately determined from UBV and uvby beta photometry and from analysis of the spectrograms: 5760 +/- 100 K for the primary and 5560 +/- 150 K for the secondary, corresponding to spectral types of G5 and G7, and 0.050 mag for interstellar reddening Eb-y. The orbits are slightly eccentric, and spectral line widths give observed rotational velocities that are not significantly different from synchronous for both components. The components of RW Lac are old, somewhat metal-deficient, low-mass, main-sequence stars with an age of about 11 Gyr, 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. Univ Fed Minas Gerais, Inst Ciencias Exatas, Dept Fis, BR-30123970 Belo Horizonte, MG, Brazil. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM clacy@uark.edu; gtorres@cfa.harvard.edu; claret@iaa.es; lpv@fisica.ufmg.br NR 49 TC 30 Z9 31 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 DEC PY 2005 VL 130 IS 6 BP 2838 EP 2846 DI 10.1086/497433 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800030 ER PT J AU Garcia-Alvarez, D Johns-Krull, CM Doyle, JG Ugarte-Urra, I Madjarska, MS Butler, CJ AF Garcia-Alvarez, D Johns-Krull, CM Doyle, JG Ugarte-Urra, I Madjarska, MS Butler, CJ TI Optical and EUV observations of solar flare kernels SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun : activity; Sun : photosphere; Sun : flares; Sun : chromosphere; line : formation; line : profiles ID WHITE-LIGHT FLARE; CORONAL DIAGNOSTIC SPECTROMETER; HIGH TIME RESOLUTION; X-RAY-BURSTS; 1982 JUNE 15; H-ALPHA; CHROMOSPHERIC EVAPORATION; STELLAR FLARES; ROTATIONAL MODULATION; MODEL CHROMOSPHERES AB We present high-resolution spectral observations, covering the entire optical region ( 3800-9000 (A) over circle), of a solar flare observed during a multiwavelength campaign. The flare, recorded on 2002 January 11, was a medium solar flare event ( GOES class C7.5). The spectral observations were carried out using the Hamilton echelle spectrograph on the coude auxiliary telescope at Lick Observatory and with the Coronal Diagnostic Spectrometer ( CDS) on board SoHO. The high signal-to-noise optical spectra are analysed using the same techniques as we applied to stellar flare data. Ha images obtained at Big Bear Solar Observatory ( BBSO), plus magnetograms obtained with the Michelson Doppler Imager ( MDI) on board SoHO and Transition Region And Coronal Explorer ( TRACE) 1600 (A) over circle were used in the flare analysis. We observe stellar-like behaviour in the main solar chromospheric activity indicators, which show either filling-in or emission during the flare. We find that the Balmer and Ca II lines show asymmetric profiles, with red-shifted wings and blue-shifted cores. This behaviour could be explained by material expanding. During the flare, the Mg I and Fe I lines show a filling-in of the line profile indicating that the flare affected the lower atmosphere. There is some evidence for pre-flare heating as seen in Fe XIX 592 (A) over circle. Furthermore, O v 629 (A) over circle shows an increase in flux some 10 min. before the coronal lines, perhaps indicating particle beam heating in the initial stages of the flare. We have also determined the main physical parameters at flare maximum. The electron densities and electron temperatures found for the flare imply that the Balmer emitting plasma originates in the chromosphere. The physical parameters obtained for the modelled flare are consistent with previously derived values for solar flares. C1 Armagh Observ, Armagh BT61 9DG, North Ireland. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. Observ Royal Belgique, Dept Solar Phys, B-1180 Brussels, Belgium. RP Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland. EM dgarcia@cfa.harvard.edu RI Ugarte-Urra, Ignacio/B-1241-2009; OI Ugarte-Urra, Ignacio/0000-0001-5503-0491 NR 78 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2005 VL 444 IS 2 BP 593 EP 603 DI 10.1051/0004-6361:20053708 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986PJ UT WOS:000233461900033 ER PT J AU Sazonov, S Churazov, E Revnivtsev, M Vikhlinin, A Sunyaev, R AF Sazonov, S Churazov, E Revnivtsev, M Vikhlinin, A Sunyaev, R TI Identification of 8 INTEGRAL hard X-ray sources with Chandra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; galaxies : Seyfert; X-rays : general AB We report the results of identification of 8 hard X-ray sources discovered by the INTEGRAL observatory during the ongoing all-sky survey. These sources have been observed by Chandra. In 6 cases a bright X-ray source was found within the INTEGRAL localization region, which permitted to unambiguously identify 5 of the objects with nearby galaxies, implying that they have an active galactic nucleus (AGN), whereas have one source is likely an X-ray binary in LMC. 4 of the 5 newly discovered AGNs have measured redshifts in the range 0.025-0.055. The X-ray spectra reveal the presence of significant amounts of absorbing gas (N-H in the range 10(22)-10(24) cm cm(-2)) in all 5 AGNs, demonstrating that INTEGRAL is starting to fill in the sample of nearby obscured AGNs. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sazonov, S (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM sazonov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 NR 11 TC 34 Z9 34 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 DEC PY 2005 VL 444 IS 2 BP L37 EP L40 DI 10.1051/0004-6361:200500205 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986PJ UT WOS:000233461900005 ER PT J AU Schroedter, M Badran, HM Buckley, JH Gordo, JB Carter-Lewis, DA Duke, C Fegan, DJ Fegan, SF Finley, JP Gillanders, GH Grube, J Horan, D Kenny, GE Kertzman, M Kosack, K Krennrich, F Kieda, DB Kildea, J Lang, MJ Lee, K Moriarty, P Quinn, J Quinn, M Power-Mooney, B Sembroski, GH Wakely, SP Vassiliev, VV Weekes, TC Zweerink, J AF Schroedter, M Badran, HM Buckley, JH Gordo, JB Carter-Lewis, DA Duke, C Fegan, DJ Fegan, SF Finley, JP Gillanders, GH Grube, J Horan, D Kenny, GE Kertzman, M Kosack, K Krennrich, F Kieda, DB Kildea, J Lang, MJ Lee, K Moriarty, P Quinn, J Quinn, M Power-Mooney, B Sembroski, GH Wakely, SP Vassiliev, VV Weekes, TC Zweerink, J TI A very high energy gamma-ray spectrum of 1ES 2344+514 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (1ES 2344+514); gamma rays : observations ID BL-LACERTAE OBJECTS; EINSTEIN SLEW SURVEY; HOST GALAXIES; MARKARIAN 421; 1ES 2344+514; CHERENKOV TELESCOPES; IMAGING TECHNIQUE; TEV ENERGIES; PKS 2155-304; CRAB-NEBULA AB The BL Lacertae (BL Lac) object 1ES 2344+514 (1ES 2344), at a redshift of 0.044, was discovered as a source of very high energy (VHE) gamma rays by the Whipple collaboration in 1995 (Catanese et al.). This detection was recently confirmed by the HEGRA collaboration (Tluczykont et al.). As is typical for high-frequency-peaked blazars, the VHE gamma-ray emission is highly variable. On the night of 1995 December 20, a gamma-ray flare of 5.3 sigma significance was detected, the brightest outburst from this object to date. The emission region is compatible with a point source. The spectrum between 0.8 and 12.6 TeV can be described by a power law, d(3)N/dEdAdt = (5.1 +/- 1.0(st) +/- 1.2(sy)) X 10(-7)(E/TeV)(-2.54 +/- 0.17st +/- 0.07sy) TeV-1 m(-2) s(-1). If we compare the spectral index with that of the other five confirmed TeV blazars, the spectrum of 1ES 2344 is similar to that of 1ES 1959+650, which is located at almost the same distance. The spectrum of 1ES 2344 is steeper than the brightest flare spectra of Markarian 421 (Mrk 421) and Markarian 501 ( Mrk 501), both of which are located at a distance about two-thirds that of 1ES 2344, and harder than the spectra of PKS 2155-304 and H1426+428, which are located almost 3 times as far away. This trend is consistent with attenuation caused by the infrared extragalactic background radiation. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Tanta Univ, Fac Sci, Dept Phys, Tanta 31527, Egypt. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland Univ Coll Dublin, Dept Expt 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. Natl Univ Ireland Univ Coll Galway, Dept Phys, Galway, Ireland. Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 6369, Amado, AZ 85645 USA. OI Lang, Mark/0000-0003-4641-4201 NR 58 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2005 VL 634 IS 2 BP 947 EP 954 DI 10.1086/496968 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700019 ER PT J AU Reiners, A Basri, G Mohanty, S AF Reiners, A Basri, G Mohanty, S TI Discovery of an M4 spectroscopic binary in Upper Scorpius: A calibration point for young low-mass evolutionary models SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; stars : fundamental parameters; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID MEASURING FUNDAMENTAL PARAMETERS; SPECTRAL ENERGY-DISTRIBUTIONS; BROWN DWARFS; SUBSTELLAR OBJECTS; STARS; DISK AB We report the discovery of a new low-mass spectroscopic (SB2) stellar binary system in the star-forming region of Upper Scorpius. This object, UScoCTIO 5, was discovered by Ardila and coworkers, who assigned it a spectral class of M4. A Keck I HIRES spectrum revealed it to be double-lined, and we then carried out a program at several observatories to determine its orbit. The orbital period is 34 days, and the eccentricity is nearly 0.3. The importance of such a discovery is that it can be used to help calibrate evolutionary models at low masses and young ages. This is one of the outstanding problems in the study of formation mechanisms and initial mass functions at low masses. The orbit allows us to place a lower limit of 0: 64 +/- 0: 02 M-circle dot on the total system mass. The components appear to be of almost equal mass. We are able to show that this mass is significantly higher than predicted by evolutionary models for an object of this luminosity and age, in agreement with other recent results. More precise determination of the temperature and surface gravity of the components would be helpful in further solidifying this conclusion. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hamburg, D-21029 Hamburg, Germany. RP Reiners, A (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. EM areiners@astron.berkeley.edu; basri@astron.berkeley.edu; smohanty@cfa.harvard.edu NR 23 TC 12 Z9 12 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP 1346 EP 1352 DI 10.1086/432878 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700053 ER PT J AU Chen, CH Patten, BM Werner, MW Dowell, CD Stapelfeldt, KR Song, I Stauffer, JR Blaylock, M Gordon, KD Krause, V AF Chen, CH Patten, BM Werner, MW Dowell, CD Stapelfeldt, KR Song, I Stauffer, JR Blaylock, M Gordon, KD Krause, V TI A Spitzer study of dusty disks around nearby, young stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation ID VEGA-LIKE STARS; MULTIBAND IMAGING PHOTOMETER; STELLAR KINEMATIC GROUPS; PICTORIS MOVING GROUP; A-TYPE STARS; SPACE-TELESCOPE; BETA-PICTORIS; DEBRIS DISKS; NORTHERN-HEMISPHERE; MASS STARS AB We have obtained Spitzer Space Telescope MIPS (Multiband Imaging Photometer for Spitzer) observations of 39A-throughM-type dwarfs, with estimated ages between 12 and 600 Myr; IRAC observations for a subset of 11 stars; and follow-up CSO SHARC II 350 mu m observations for a subset of two stars. None of the objects observed with IRAC possess infrared excesses at 3.6 - 8.0 mu m; however, seven objects observed with MIPS possess 24 and/or 70 mu m excesses. Four objects ( k Phe, HD 92945, HD 119124, and AU Mic), with estimated ages 12 - 200 Myr, possess strong 70 mu m excesses, >= 100% larger than their predicted photospheres, and no 24 mu m excesses, suggesting that the dust grains in these systems are cold. One object ( HD 112429) possesses moderate 24 and 70 mu m excesses with a color temperature, T-gr = 100K. Two objects (alpha(1)Lib and HD 177724) possess such strong 24 mu m excesses that their 12, 24, and 70 mu m fluxes cannot be self-consistently modeled using a modified blackbody despite a 70 mu m excess > 2 times greater than the photosphere around alpha(1)Lib. The strong 24 mu m excesses may be the result of emission in spectral features, as observed toward the Hale-Bopp star HD 69830. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Gemini Observ, Hilo, HI 96720 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Chen, CH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Stapelfeldt, Karl/D-2721-2012 NR 63 TC 82 Z9 82 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 DEC 1 PY 2005 VL 634 IS 2 BP 1372 EP 1384 DI 10.1086/497124 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700055 ER PT J AU Mamajek, EE AF Mamajek, EE TI A moving cluster distance to the exoplanet 2M1207b in the TW Hydrae association SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (TW Hydrae); planetary systems; stars : distances; stars : individual (2MASSW J1207334-393254); stars : kinematics; stars : low-mass, brown dwarfs ID SCORPIO-CENTAURUS ASSOCIATION; ASTROMETRIC RADIAL-VELOCITIES; ETA-CHAMAELEONTIS CLUSTER; EXTRASOLAR GIANT PLANETS; CONVERGENT-POINT METHOD; YOUNG BROWN DWARF; LOW-MASS STARS; TAURI STARS; INTERSTELLAR CLOUDS; EVOLUTIONARY MODELS AB A candidate extrasolar planet companion to the young brown dwarf 2MASSW J1207334 - 393254 ( hereafter 2M1207) was recently discovered by Chauvin et al. They find that the temperature and luminosity of 2M1207b are consistent with a young, similar to 5MJ planet. The 2M1207 system is purported to be a member of the TW Hya association (TWA) and situated similar to 70 pc away. Using a revised space motion vector for TWA and improved proper motion for 2M1207, I use the moving cluster method to estimate the distance to the 2M1207 system and other TWA members. The derived distance for 2M1207 ( 53 +/- 6 pc) forces the brown dwarf and planet to be half as luminous as previously thought. The inferred masses for 2M1207A and 2M1207b decrease to similar to 21 and similar to 3 - 4M(J), respectively, with the mass of 2M1207b well below the observed tip of the planetary mass function and the theoretical deuterium-burning limit. After removing probable Lower Centaurus Crux ( LCC) members from the TWA sample, as well as the probable nonmember TWA22, the remaining TWA membership is found to have distances of 49 - 3 ( s: e: m:) +/- 12 ( 1 sigma) pc and an internal one-dimensional velocity dispersion of 0.8(-0.2)(+0.3) km s(-1). There is weak evidence that the TWA is expanding, and the data are consistent with a lower limit on the expansion age of 10 Myr ( 95% confidence). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. EM emamajek@cfa.harvard.edu NR 77 TC 137 Z9 138 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 DEC 1 PY 2005 VL 634 IS 2 BP 1385 EP 1394 DI 10.1086/468181 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700056 ER PT J AU Beuther, H Sridharan, TK Saito, M AF Beuther, H Sridharan, TK Saito, M TI Caught in the act: The onset of massive star formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : early-type; stars : formation; stars : individual (IRDC 18223-3); stars : winds, outflows ID SPITZER-SPACE-TELESCOPE; PROTOSTELLAR CANDIDATES; HII-REGIONS; CLOUD CORES; COLD CORES; OUTFLOWS; EXTINCTION; CONTINUUM; SAMPLE AB Combining mid-infrared data from the Spitzer Space Telescope with cold gas and dust emission observations from the Plateau de Bure Interferometer, we characterize the infrared dark cloud IRDC 18223-3 at high spatial resolution. The millimeter continuum data reveal a massive similar to 184 M, gas core with a projected size of similar to 28,000 AU that has no associated protostellar mid-infrared counterpart. However, the detection of 4.5 mm emission at the edge of the core indicates early outflow activity, which is supported by broad CO and CS spectral line-wing emission. Moreover, systematically increasing N2H+(1-0) line width toward the millimeter core center can be interpreted as additional evidence for early star formation. Furthermore, the N2H+(1-0) line emission reveals a less massive secondary core that could be in an evolutionary stage prior to any star formation activity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu; tksridha@cfa.harvard.edu; masao.saito@nao.ac.jp NR 26 TC 56 Z9 56 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L185 EP L188 DI 10.1086/498867 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000016 ER PT J AU Humphreys, EML Greenhill, LJ Reid, MJ Beuther, H Moran, JM Gurwell, M Wilner, DJ Kondratko, PT AF Humphreys, EML Greenhill, LJ Reid, MJ Beuther, H Moran, JM Gurwell, M Wilner, DJ Kondratko, PT TI First detection of millimeter/submillimeter extragalactic H2O maser emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual ( NGC 3079); galaxies : nuclei; masers; submillimeter; techniques : high angular resolution ID SUBMILLIMETER WATER MASERS; ACTIVE GALACTIC NUCLEI; SPIRAL GALAXY NGC-3079; MILLIMETER ARRAY; ACCRETION DISK; PARSEC REGION; H2O EMISSION; NGC 3079; STARS; TORUS AB We report the first detection of an extragalactic millimeter wavelength H2O maser at 183 GHz toward NGC 3079 using the Submillimeter Array ( SMA) and a tentative submillimeter wave detection of the 439 GHz maser toward the same source using the James Clerk Maxwell Telescope ( JCMT). These H2O transitions are known to exhibit maser emission in star-forming regions and evolved stars. NGC 3079 is a well-studied nuclear H2O maser source at 22 GHz with a time-variable peak flux density in the range 3-12 Jy. The 183 GHz H2O maser emission, with a peak flux density of similar to 0.5 Jy ( 7 sigma detection), also originates from the nuclear region of NGC 3079 and is spatially coincident with the dust continuum peak at 193 GHz ( 53 mJy integrated). Peak emission at both 183 and 439 GHz occurs in the same range of velocity as that covered by the 22 GHz spectrum. We estimate the gas-to-dust ratio of the nucleus of NGC 3079 to be approximate to 150, comparable to the Galactic value of 160. Discovery of maser emission in an active galactic nucleus beyond the long-known 22 GHz transition opens the possibility of future position-resolved radiative transfer modeling of accretion disks and outflows <1 pc from massive black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Humphreys, EML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ehumphreys@cfa.harvard.edu; lgreenhill@cfa.harvard.edu; mreid@cfa.harvard.edu; hbeuther@cfa.harvard.edu; jmoran@cfa.harvard.edu; mgurwell@cfa.harvard.edu; dwilner@cfa.harvard.edu; pkondratko@cfa.harvard.edu NR 45 TC 14 Z9 14 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L133 EP L136 DI 10.1086/498890 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000003 ER PT J AU Marsden, SC Berdyugina, SV Donati, JF Eaton, JA Williamson, MH Ilyin, I Fischer, DA Munoz, M Isaacson, H Ratner, MI Semel, M Petit, P Carter, BD AF Marsden, SC Berdyugina, SV Donati, JF Eaton, JA Williamson, MH Ilyin, I Fischer, DA Munoz, M Isaacson, H Ratner, MI Semel, M Petit, P Carter, BD TI A sun in the spectroscopic binary IM Pegasi, the guide star for the Gravity Probe B mission SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : individual (IM Pegasi) ID ACTIVE STARS; PARAMETERS; PRECISION AB We present the first detection of the secondary of the spectroscopic binary system IM Pegasi (HR 8703), the guide star for the NASA-Stanford relativity gyroscope mission Gravity Probe B. In support of this mission, high-resolution echelle spectra of IM Peg have been obtained on an almost nightly basis. Applying the technique of least-squares deconvolution, we achieve very high signal-to-noise ratio line profiles and detect the orbit of the secondary of the system. Combining almost 700 new radial velocity measurements of both the primary and secondary of the system with previous measurements, we derive improved orbital parameters of the IM Peg system. Using these estimates along with the previously determined range of orbital inclination angles for the system, we find that the primary of IM Peg is a giant of mass 1.8 +/- 0.2 M-circle dot while the secondary is a dwarf of mass 1.0 +/- 0.1 M-circle dot. C1 ETH Zentrum, Inst Astron, CH-8092 Zurich, Switzerland. Univ Oulu, Dept Phys Sci, Astron Div, FI-90014 Oulu, Finland. Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. Inst Astrophys, D-14482 Potsdam, Germany. San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, Lab Etudes Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. Univ So Queensland, Fac Sci, Toowoomba, Qld 4350, Australia. RP Marsden, SC (reprint author), ETH Zentrum, Inst Astron, CH-8092 Zurich, Switzerland. EM marsden@astro.phys.ethz.ch RI Petit, Pascal/C-5842-2011; OI Marsden, Stephen/0000-0001-5522-8887; Petit, Pascal/0000-0001-7624-9222 NR 16 TC 14 Z9 14 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L173 EP L176 DI 10.1086/498941 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000013 ER PT J AU Grimm, HJ McDowell, J Zezas, A Kim, DW Fabbiano, G AF Grimm, HJ McDowell, J Zezas, A Kim, DW Fabbiano, G TI The X-ray binary population in M33. I. Source list and luminosity function SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : individual (M33, NGC 598) ID CHANDRA MULTIWAVELENGTH PROJECT; EVOLVED MASSIVE STARS; POINT-SOURCE CATALOGS; ROSAT HRI CATALOG; SPIRAL GALAXY M33; LOCAL GROUP; NEARBY GALAXIES; CONFIDENCE-LIMITS; RED SUPERGIANTS; M-33 AB In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of similar to 0.2 deg(2) down to a flux limit of 3 x 10(-16) ergs s(-1) cm(-2), which corresponds to a luminosity of similar to 2 x 10(34) ergs s(-1) at a distance of 840 kpc. From the source list we construct the luminosity functions of sources observed in M33. If we take into account background contamination, the luminosity functions are consistent with those of other star-forming galaxies. In addition, the combination of X-ray color analysis and the existence of "blue" optical counterparts strongly indicates that the X-ray point-source population in M33 consists of young objects. Above 3 x 10(35) ergs s(-1) there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grimm, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 53 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 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2005 VL 161 IS 2 BP 271 EP 303 DI 10.1086/468185 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CO UT WOS:000233930500004 ER PT J AU Zhao, P Grindlay, JE Hong, JS Laycock, S Koenig, XP Schlegel, EM van den Berg, M AF Zhao, P Grindlay, JE Hong, JS Laycock, S Koenig, XP Schlegel, EM van den Berg, M TI ChaMPlane Optical Survey: Mosaic photometry SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE surveys; X-rays : general ID DIGITAL SKY SURVEY; CATACLYSMIC VARIABLES; GALACTIC-CENTER; EMISSION; STARS AB The Chandra Multiwavelength Plane (ChaMPlane) survey to identify and analyze the serendipitous X-ray sources in deep Galactic plane fields incorporates the ChaMPlane Optical Survey, which is one of NOAO's Longterm Survey Programs. We started this optical imaging survey in 2000 March and completed it in 2005 June. Using the NOAO 4 m telescopes with the Mosaic cameras at CTIO and KPNO, deep images of the ChaMPlane fields are obtained in V, R, I, and H alpha bands. This paper describes the process of observation, data reduction, and analysis of fields included in the ChaMPlane Optical Survey and describes the search for H alpha emission objects and Chandra optical counterparts. We illustrate these procedures using the ChaMPlane field for the black hole X-ray binary GROJ 0422+32 as an example. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zhao@cfa.harvard.edu OI Koenig, Xavier/0000-0002-9478-4170 NR 19 TC 20 Z9 20 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 DEC PY 2005 VL 161 IS 2 BP 429 EP 443 DI 10.1086/497095 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CO UT WOS:000233930500008 ER PT J AU de Queiroz, K AF de Queiroz, K TI Different species problems and their resolution SO BIOESSAYS LA English DT Article ID ESSENTIALISM; TAXONOMY; BIOLOGY; STASIS AB At least three different issues are commonly referred to by the term "the species problem": one concerns the necessary properties of species, a second the processes responsible for the existence of species, and a third methods for inferring species limits. Solutions have recently been proposed to the first two problems, which are conceptual in nature (the third is methodological). The first equates species with metapopulation lineages and proposes that existence as a separately evolving metapopulation lineage be considered the only necessary property of species. The second views the species category as a cluster concept and proposes that no single process or set of processes be considered necessary for the existence of species. Although these two solutions have been portrayed as being in conflict, they are, in fact, highly compatible. Moreover, the proposals in question clarify the problem concerning methods for inferring the limits of species, which has fora long time been confused with the problem concerning the necessary properties of species. Together these proposals provide the opportunity for biology to move beyond debates about the definition of the species category and focus on estimating the boundaries and numbers of species as well as studying the diverse processes involved in their origin and persistence. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP de Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM dequeirk@si.edu NR 46 TC 100 Z9 104 U1 2 U2 37 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0265-9247 J9 BIOESSAYS JI Bioessays PD DEC PY 2005 VL 27 IS 12 BP 1263 EP 1269 DI 10.1002/bies.20325 PG 7 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 990TW UT WOS:000233767100008 PM 16299765 ER PT J AU Harrison, RD AF Harrison, RD TI Figs and the diversity of tropical rainforests SO BIOSCIENCE LA English DT Article DE biodiversity; Ficus; rare niches; species coexistence; tropical rainforest ID KEYSTONE PLANT RESOURCE; PAPUA-NEW-GUINEA; EMERGENT ISLAND; CALDERA LAKE; LONG-ISLAND; FICUS; MUTUALISM; MORACEAE; TREE; DIVERSIFICATION AB Ficus (Moraceae) is arguably one of the most important plant genera in lowland tropical rainforests. A brief review of tropical florulas also demonstrates that Ficus is the only ubiquitously diverse genus in lowland rainforests. Monoecious hemi-epiphytic figs, constituting independent radiations in each tropical biome, make up a significant proportion of species everywhere, but in Asia dioecious figs have diversified into a variety of niches, making the assemblages of this region especially speciose. Pioneer attributes have endowed figs with tremendous evolutionary flexibility, while long-range seed dispersal ensures that a high proportion of the regional species pool is represented in local assemblages. Large numbers of Ficus species are able to coexist because many are extremely rare as a result of limited recruitment opportunities, which limits competition. They are nevertheless able to breed at low densities because they possess an efficient, long-range pollination system. These factors are likely to be important in the diversity of other plant groups in the tropics. C1 Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Harrison, RD (reprint author), Res Inst Human & Nat, Kamikyo Ku, Takashima Cho 335, Kyoto, Japan. EM rhett@chikyu.ac.jp NR 52 TC 96 Z9 101 U1 5 U2 45 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD DEC PY 2005 VL 55 IS 12 BP 1053 EP 1064 DI 10.1641/0006-3568(2005)055[1053:FATDOT]2.0.CO;2 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 992BH UT WOS:000233858400007 ER PT J AU Gamon, JA Kitajima, K Mulkey, SS Serrano, L Wright, SJ AF Gamon, JA Kitajima, K Mulkey, SS Serrano, L Wright, SJ TI Diverse optical and photosynthetic properties in a neotropical dry forest during the dry season: Implications for remote estimation of photosynthesis SO BIOTROPICA LA English DT Article DE APAR; biodiversity; canopyo crane; normalized difference vegetation index (NDVI); photosynthetic downregulation; photochemical reflectance index (PRI); radiation-use efficiency; tropical dry forest; xanthophyll cycle ID RADIATION-USE EFFICIENCY; LIGHT-USE EFFICIENCY; SPECTRAL REFLECTANCE; TROPICAL FOREST; VEGETATION INDEX; ATMOSPHERIC CO2; CARBON-DIOXIDE; BOREAL FOREST; CANOPY TREES; TRANSPIRATION AB Using optical and photosynthetic assays from a canopy access crane, we examined the Photosynthetic performance of tropical dry forest canopies during the (it), season in Parque Metropolitano, Panama City, Panama. Photosynthetic gas exchange, chlorophyll fluorescence, and three indices derived from spectra] reflectance (the normalized difference vegetation index, the simple ratio, and the photochemical reflectance index) were used as indicators of structural and physiological components of photosynthetic activity. Considerable interspecific variation was evident in structural and physiological behavior in this forest stand, which included varying degrees of foliage loss, altered leaf orientation, stomatal closure, and phorosystem 11 downregulation. The normalized difference vegetation index and the simple ratio were closely related to canopy structure and absorbed radiation for most species, but failed to capture the widely divergent Photosynthetic behavior among evergreen species exhibiting various degrees of downregulation. The photochemical reflectance index and chlorophyll fluorescence were related indicators of Photosynthetic downregulation, which was not detectable with the normalized difference vegetation index or simple ratio. These results suggest that remote sensing methods that ignore downregulation cannot capture within-stand variability ill actual carbon flux for this diverse forest type. Instead, these findings support a sampling approach that derives Photosynthetic fluxes from a consideration of both canopy light absorption (e.g., normalized difference vegetation index) and photosynthetic light-use efficiency (e.g., photochemical reflectance index). Such sampling should improve our understanding of controls on photosynthetic carbon uptake in diverse tropical forest stands. C1 Calif State Univ Los Angeles, CEA, CREST, Los Angeles, CA 90032 USA. Calif State Univ Los Angeles, Dept Biol Sci, Los Angeles, CA 90032 USA. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Dept Engn Agroalimentaria Biotecnol, Castelldefels 08860, Spain. Smithsonian Trop Res Inst, Balboa, Panama. RP Gamon, JA (reprint author), Calif State Univ Los Angeles, CEA, CREST, 5151 State Univ Dr, Los Angeles, CA 90032 USA. EM jgamon@calstatela.edu RI Kitajima, Kaoru/E-8877-2012; Serrano, Lydia/K-6731-2013; Gamon, John/A-2641-2014; Wright, Stuart/M-3311-2013; OI Gamon, John/0000-0002-8269-7723; Wright, Stuart/0000-0003-4260-5676; Serrano, Lydia/0000-0003-3776-3370 NR 62 TC 16 Z9 22 U1 1 U2 17 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 2005 VL 37 IS 4 BP 547 EP 560 DI 10.1111/j.1744-7429.2005.00072.x PG 14 WC Ecology SC Environmental Sciences & Ecology GA 990TT UT WOS:000233766800007 ER PT J AU Wang, W Potts, R Hou, YM Chen, YF Wu, HY Yuan, BY Huang, WW AF Wang, W Potts, R Hou, YM Chen, YF Wu, HY Yuan, BY Huang, WW TI Early Pleistocene hominid teeth recovered in Mohui cave in Bubing Basin, Guangxi, South China SO CHINESE SCIENCE BULLETIN LA English DT Article DE Mohui cave; hominid teeth; stone artifact; mammalian fauna; early Pleistocene ID HOMO; ASIA AB Two hominid teeth recovered in Mohui cave are morphologically distinguished from Australopithecus in Africa, but close to Homo erectus in China. These teeth are therefore provisionally assigned to Homo erectus. The associated mammalian fauna include Gigantopithecus blacki, Nestotitherium sp., Sus xiaozhu, Sus peii and Ailuropoda microta, which are typical early Pleistocene taxa in South China. The general characteristics of the Mohui faunal assemblage are similar to the Longgupo site, which is dated to 2 Ma, implying a contemporaneity for the two sites. To date, compared with the discoveries in Africa, far fewer early Pleistocene hominid fossils have been recovered in Asia, and there are intensive controversies concerning their stratigraphic provenience and typological and temporal positions. The hominid fossils from Mohui cave, with their reliable biostratigraphic positions and distinct typological features, provide important evidence regarding the issue of early human origins and evolution. C1 China Univ Geosci, Fac Earth Sci, Wuhan 430074, Peoples R China. Nat Hist Museum Guangxi Zhuang Autonomous Reg, Nanning 530012, Peoples R China. Smithsonian Inst, Museum Hist Nat, Human Origins Program, Washington, DC 20560 USA. Chinese Acad Sci, Inst Vertebrate Paleontol & Paleoanthropol, Beijing 100044, Peoples R China. Chinese Acad Sci, Inst Geol & Geophys, Beijing 100029, Peoples R China. RP Wang, W (reprint author), China Univ Geosci, Fac Earth Sci, Wuhan 430074, Peoples R China. EM wang-wei@public.nn.gx.cn NR 15 TC 28 Z9 31 U1 1 U2 7 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1001-6538 J9 CHINESE SCI BULL JI Chin. Sci. Bull. PD DEC PY 2005 VL 50 IS 23 BP 2777 EP 2782 DI 10.1360/982004-614 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 014CW UT WOS:000235457300019 ER EF