FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Sasaki, M Plucinsky, PP Gaetz, TJ Smith, RK Edgar, RJ Slane, PO AF Sasaki, M Plucinsky, PP Gaetz, TJ Smith, RK Edgar, RJ Slane, PO TI XMM-Newton observations of the Galactic supernova remnant CTB 109 (G109.1-1.0) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (CTB 109); shock waves; supernova remnants; X-rays : individual (CTB 109) ID X-RAY PULSAR; LARGE-MAGELLANIC-CLOUD; INTERSTELLAR CLOUDS; 1E 2259+586; MOLECULAR CLOUDS; BLAST WAVES; CHANDRA OBSERVATIONS; CO OBSERVATIONS; NOVA REMNANTS; CASSIOPEIA-A AB We present the analysis of the X-ray Multimirror Mission (XMM-Newton) European Photon Imaging Camera (EPIC) data of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0). CTB 109 is associated with the anomalous X-ray pulsar (AXP) 1E 2259+586 and has an unusual semicircular morphology in both the X-ray and the radio and an extended X-ray bright interior region known as the "Lobe.'' The deep EPIC mosaic image of the remnant shows no emission toward the west where a giant molecular cloud complex is located. No morphological connection between the Lobe and the AXP is found. We find remarkably little spectral variation across the remnant given the large intensity variations. All spectra of the shell and the Lobe are well fitted by a single-temperature nonequilibrium ionization model for a collisional plasma with solar abundances [kTapproximate to0.5-0.7 keV, tau=integral n(e) dt approximate to(1-4)x10(11) s cm(-3), N(H)approximate to(5-7)x10(21) cm(-2)]. There is no indication of nonthermal emission in the Lobe or the shell. We conclude that the Lobe originated from an interaction of the SNR shock wave with an interstellar cloud. Applying the Sedov solution for the undisturbed eastern part of the SNR and assuming full equilibration between the electrons and ions behind the shock front, the SNR shock velocity is derived as v(s)=720+/-60 km s(-1), the remnant age as t=(8.8+/-0.9)x10(3)d(3) yr, the initial energy as E-0=(7.4+/-2.9)x10(50) d(3)(2.5) ergs, and the preshock density of the nuclei in the ambient medium as n(0)=(0.16+/-0.02)d(3)(-0.5) cm(-3), at an assumed distance of D=3.0d(3) kpc. Assuming that CTB 109 and 1E 2259+586 are associated, these values constrain the age and the environment of the progenitor of the SNR and the pulsar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sasaki, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msasaki@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016 OI Sasaki, Manami/0000-0001-5302-1866 NR 77 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 2004 VL 617 IS 1 BP 322 EP 338 DI 10.1086/425353 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700022 ER PT J AU Muzerolle, J D'Alessio, P Calvet, N Hartmann, L AF Muzerolle, J D'Alessio, P Calvet, N Hartmann, L TI Magnetospheres and disk accretion in herbig Ae/Be stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : emission-line, Be; stars : pre-main-sequence ID T-TAURI STARS; BETA-PICTORIS PHENOMENON; UX-ORIONIS; YOUNG OBJECTS; AB-AURIGAE; CIRCUMSTELLAR DISKS; EMISSION-LINES; AE STARS; MODELS; DUST AB We present evidence of magnetically mediated disk accretion in Herbig Ae/Be stars. Magnetospheric accretion models of Balmer and sodium profiles calculated with appropriate stellar and rotational parameters are in qualitative agreement with the observed profiles of the Herbig Ae star UX Ori and yield a mass accretion rate of similar to 10(-8) M-. yr(-1). If more recent indications of an extremely large rotation rate for this object are correct, the magnetic field geometry must deviate from that of a standard dipole in order to produce line emission consistent with observed flux levels. Models of the associated accretion shock qualitatively explain the observed distribution of excess fluxes in the Balmer discontinuity for a large ensemble of Herbig Ae/Be stars and imply typically small mass accretion rates, less than or similar to10(-7) M-. yr(-1). In order for accretion to proceed onto the star, significant amounts of gas must exist inside the dust destruction radius, which is potentially problematic for recently advocated scenarios of "puffed'' inner dust wall geometries. However, our models of the inner gas disk show that for the typical accretion rates we have derived, the gas should generally be optically thin, thus allowing direct stellar irradiation of the inner dust edge of the disk. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 65 TC 147 Z9 147 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 406 EP 417 DI 10.1086/425260 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700028 ER PT J AU Di Francesco, J Andre, P Myers, PC AF Di Francesco, J Andre, P Myers, PC TI Quiescent dense gas in protostellar clusters: The Ophiuchus a core SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : individual (Ophiuchus A); ISM : kinematics and dynamics; stars : formation ID MAGNETIZED MOLECULAR CLOUDS; STAR-FORMATION; RHO-OPHIUCHI; DARK CLOUDS; SCORPIO-CENTAURUS; PRESTELLAR CORES; N2H+; KINEMATICS; OUTFLOW; AMMONIA AB We present combined BIMA interferometer and IRAM 30 m telescope data of N2H+ 1-0 line emission across the nearby dense star-forming core Ophiuchus A at high linear resolution (e.g., similar to 1000 AU). Six maxima of integrated line intensity are detected, which we designate Oph A-N1 through N6. The N4 and N5 maxima coincide with the starless continuum objects SM1 and SM2, respectively, but the other maxima do not coincide with previously identified objects. In contrast, relatively little (NH+)-H-2 1 - 0 emission coincides with the starless object SM2 and the Class 0 protostar VLA 1623. The FWHM of the N2H+ 1 - 0 line, DeltaV, varies by a factor of similar to 5 across Oph A. Values of DeltaV < 0.3 km s(-1) are found in 14 locations in Oph A, but only that associated with N6 is both well defined spatially and larger than the beam size. Centroid velocities of the line, V-LSR, vary relatively little, having an rms of only similar to 0.17 km s(-1). Small-scale V-LSR gradients of less than 0.5 km s(-1) over similar to 0.01 pc are found near SM1, SM1N, and SM2 but not N6. The low N2H+ abundances of SM2 or VLA 1623 relative to SM1, SM1N, or N6 may reflect relatively greater amounts of N-2 adsorption onto dust grains in their colder and probably denser interiors. The low Delta V of N6, i.e., 0.193 km s(-1) FWHM, is only marginally larger than the FWHM expected from thermal motions alone, suggesting that turbulent motions in the Oph A core have been reduced dramatically at this location. The nondetection of N6 in previous thermal continuum maps suggests that interesting sites possibly related to star formation may be overlooked in such data. C1 Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Ctr Etud Saclay, DAPNIA, DSM, CEA,Serv Astrophys, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. NR 63 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 10 PY 2004 VL 617 IS 1 BP 425 EP 438 DI 10.1086/425264 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700030 ER PT J AU Povich, MS Raymond, JC Lobel, A Menou, K AF Povich, MS Raymond, JC Lobel, A Menou, K TI Far Ultraviolet Spectroscopic Explorer observations of the dwarf nova SW Ursae Majoris during quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; novae, cataclysmic variables; stars : individual (SW Ursae Majoris); ultraviolet : stars ID HUBBLE-SPACE-TELESCOPE; X-RAY; H-2 EMISSION; WZ SAGITTAE; ACCRETION DISKS; 2001 OUTBURST; WHITE-DWARF; T-TAURI; INSTABILITY; SPECTRUM AB We present spectroscopic observations of the short-period cataclysmic variable SW UMa obtained by the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite while the system was in quiescence. The data include the resonance lines of O vi at 1031.91 and 1037.61 Angstrom. These lines are present in emission, and they exhibit both narrow (similar to 150 km s(-1)) and broad (similar to 2000 km s(-1)) components. The narrow O vi emission lines exhibit unusual double-peaked and redshifted profiles. We attribute the source of this emission to a cooling flow onto the surface of the white dwarf primary. The broad O vi emission most likely originates in a thin, photoionized surface layer on the accretion disk. We searched for emission from H-2 at 1050 and 1100 Angstrom, motivated by the expectation that the bulk of the quiescent accretion disk is in the form of cool, molecular gas. If H2 is present, then our limits on the fluxes of the H-2 lines are consistent with the presence of a surface layer of atomic H that shields the interior of the disk. These results may indicate that accretion operates primarily in the surface layers of the disk in SW UMa. We also investigate the far-UV continuum of SW UMa and place an upper limit of 15,000 K on the effective temperature of the white dwarf. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Povich, MS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 41 TC 1 Z9 1 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 2004 VL 617 IS 1 BP 500 EP 507 DI 10.1086/425213 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700036 ER PT J AU Testa, P Drake, JJ Peres, G AF Testa, P Drake, JJ Peres, G TI The density of coronal plasma in active stellar coronae SO ASTROPHYSICAL JOURNAL LA English DT Review DE plasmas; stars : activity; stars : coronae; stars : late-type; Sun : corona; X-rays : stars ID X-RAY SPECTROSCOPY; RS-CANUM-VENATICORUM; HELIUM-LIKE IONS; EXTREME-ULTRAVIOLET-EXPLORER; XMM-NEWTON VIEW; LATE-TYPE STARS; GUIDANCE SENSOR 3; BINARY II PEGASI; T-TAURI STARS; ALPHA-CEN-A AB We have analyzed high-resolution X-ray spectra of a sample of 22 active stars observed with the High Energy Transmission Grating Spectrometer on Chandra in order to investigate their coronal plasma density. Densities were investigated using the lines of the He-like ions O VII, Mg xi, and Si XIII. Si XIII lines in all stars of the sample are compatible with the low-density limit (i.e., ne less than or similar to10(13) cm(-3)), casting some doubt on results based on lower resolution Extreme Ultraviolet Explorer (EUVE) spectra finding densities n(e) > 10(13) cm(-3). Mg XI lines betray the presence of high plasma densities up to a few times 10(12) cm(-3) for most of the sources with higher X-ray luminosity (greater than or similar to10(30) ergs s(-1)); stars with higher L-X and L-X/L-bol tend to have higher densities at high temperatures. Ratios of O VII lines yield much lower densities of a few times 10(10) cm(-3), indicating that the "hot'' and "cool'' plasma resides in physically different structures. In the cases of EV Lac, HD 223460, Canopus, mu Vel, TY Pyx, and IM Peg, our results represent the first spectroscopic estimates of coronal density. No trends in density-sensitive line ratios with stellar parameters effective temperature and surface gravity were found, indicating that plasma densities are remarkably similar for stars with pressure scale heights differing by up to 3 orders of magnitude. Our findings imply remarkably compact coronal structures, especially for the hotter (similar to7 MK) plasma emitting the Mg xi lines characterized by the coronal surface filling factor, f(Mg xi), ranging from 10(-4) to 10(-1), while we find f(O vii) values from a few times 10(-3) up to similar to1 for the cooler (similar to2 MK) plasma emitting the O vii lines. We find that fO vii approaches unity at the same stellar surface X-ray flux level as characterizes solar active regions, suggesting that these stars become completely covered by active regions. At the same surface flux level, fMg xi is seen to increase more sharply with increasing surface flux. These results appear to support earlier suggestions that hot 10(7) K plasma in active coronae arises from flaring activity and that this flaring activity increases markedly once the stellar surface becomes covered with active regions. Comparison of our measured line fluxes with theoretical models suggests that significant residual model inaccuracies might be present and, in particular, that cascade contributions to forbidden and intercombination lines resulting from dielectronic recombination might be to blame. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. RP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. EM ptesta@head.cfa.harvard.edu; jdrake@head.cfa.harvard.edu; peres@astropa.unipa.it OI PERES, Giovanni/0000-0002-6033-8180 NR 109 TC 78 Z9 78 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2004 VL 617 IS 1 BP 508 EP 530 DI 10.1086/422355 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700037 ER PT J AU Luhman, KL Peterson, DE Megeath, ST AF Luhman, KL Peterson, DE Megeath, ST TI Spectroscopic confirmation of the least massive known brown dwarf in Chamaeleon SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID STAR-FORMING REGION; I DARK CLOUD; INFRARED SPECTRAL CLASSIFICATION; MAIN-SEQUENCE STARS; MOLECULAR CLOUD; EVOLUTIONARY MODELS; YOUNG STELLAR; CANDIDATES; CENSUS; CORE AB We present spectroscopy of two candidate substellar members of the Chamaeleon I star-forming region. The candidates, which were identified photometrically by Oasa, Tamura, & Sugitani, have been observed at 1 - 2.5 mum during commissioning of the Gemini Near-Infrared Spectrograph. The late-type nature of one of the candidates, OTS 44, is confirmed through the detection of strong steam absorption bands. The other object, OTS 7, exhibits no late-type features and is likely a background star or galaxy. The gravity-sensitive shape of the H and K band continua demonstrate that OTS 44 is a young, pre-main-sequence object rather than a field dwarf. We measure a spectral type of M9.5 for OTS 44 based on a comparison of its spectrum to data for optically classified young late-type objects. Because OTS 44 is the coolest and faintest object with confirmed membership in Cha I, it is very likely the least massive known member of the cluster. By comparing the position of OTS 44 on the H-R diagram to the evolutionary models of Chabrier & Baraffe, we infer a mass of similar to 0.015 M-.. Although this estimate is uncertain by at least a factor of 2, OTS 44 is nevertheless one of the least massive free-floating brown dwarfs confirmed spectroscopically to date. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu; dawnp@astro.pas.rochester.edu; tmegeath@cfa.harvard.edu NR 37 TC 37 Z9 37 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 2004 VL 617 IS 1 BP 565 EP 568 DI 10.1086/425228 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CP UT WOS:000225766700041 ER PT J AU Braatz, JA Henkel, C Greenhill, LJ Moran, JM Wilson, AS AF Braatz, JA Henkel, C Greenhill, LJ Moran, JM Wilson, AS TI A green bank telescope search for water masers in nearby active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; galaxies : Seyfert; ISM : molecules; masers; radio lines : galaxies ID SEYFERT-2 GALAXY NGC-4388; H2O MASER; IRAS GALAXIES; EMISSION; DISCOVERY; NGC-4258; DISK; MEGAMASERS; GAS; VELOCITIES AB Using the Green Bank Telescope, we have conducted a survey for 1.3 cm water maser emission toward the nuclei of nearby active galaxies, the most sensitive large survey for H2O masers to date. Among 145 galaxies observed, maser emission was newly detected in 11 sources and confirmed in one other. Our survey targeted nearby (v < 12,000 km s(-1)), mainly type 2 active galactic nuclei (AGNs) north of δ = -20&DEG; and includes a few additional sources as well. We find that more than one-third of Seyfert 2 galaxies have strong maser emission, although the detection rate declines beyond v &SIM; 5000 km s(-1) because of sensitivity limits. Two of the masers discovered during this survey are found in unexpected hosts: NGC 4151 ( Seyfert 1.5) and NGC 2782 (starburst). We discuss the possible relations between the large X-ray column to NGC 4151 and a possible hidden AGN in NGC 2782 to the detected masers. Four of the masers discovered here, NGC 591, NGC 4388, NGC 5728, and NGC 6323, have high-velocity lines symmetrically spaced about the systemic velocity, a likely signature of molecular gas in a nuclear accretion disk. The maser source in NGC 6323, in particular, reveals the classic spectrum of a "disk maser" represented by three distinct groups of Doppler components. Future single-dish and VLBI observations of these four galaxies could provide a measurement of the distance to each galaxy and of the Hubble constant, independent of standard candle calibrations. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Braatz, JA (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. OI Moran, James/0000-0002-3882-4414 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 DEC 10 PY 2004 VL 617 IS 1 BP L29 EP L32 DI 10.1086/427185 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CQ UT WOS:000225766800008 ER PT J AU Kong, AKH Di Stefano, R Yuan, F AF Kong, AKH Di Stefano, R Yuan, F TI Evidence of an intermediate-mass black hole: Chandra and XMM-Newton observations of the ultraluminous supersoft X-ray source in M101 during its 2004 outburst SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M101); X-rays : binaries; X-rays : galaxies ID SOURCE POPULATION; WHITE-DWARF; GALAXY; DISCOVERY; EMISSION; SPECTRA; CAL-87 AB We report the results of Chandra and XMM-Newton observations of a new outburst of an ultraluminous supersoft X-ray source in M101. CXOU J140332.3 + 542103 was observed in a low-luminosity state (L-X similar to 10(37) ergs s(-1)) between 2004 January and May. The low-state X-ray spectra were relatively hard; the combined low-state spectrum can be fitted with a combination of a power law with photon index of 1.4 and a blackbody of 63 eV. During 2004 July, the source underwent a strong outburst and the peak 0.3 - 7 keV luminosity reached 3 x 10(40) ergs s(-1), with a bolometric luminosity of about 10(41) ergs s(-1). The outburst spectra were very soft and can be generally fitted with a blackbody model with temperatures of 50 - 100 eV. In two of the observations, absorption edges at 0.33, 0.56, 0.66, and 0.88 keV were found. An XMM-Newton observation was also performed during the decay of the outburst, and a power-law tail was seen in addition to the supersoft spectrum. We consider different accretion models; one involving an intermediate-mass black hole can explain the observations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akong@cfa.harvard.edu NR 33 TC 46 Z9 47 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 DEC 10 PY 2004 VL 617 IS 1 BP L49 EP L52 DI 10.1086/427025 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 880CQ UT WOS:000225766800013 ER PT J AU Holbrook, LT Lucas, SG Emry, RJ AF Holbrook, LT Lucas, SG Emry, RJ TI Skulls of the eocene perissodactyls (Mammalia) Homogalax and Isectolophus SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID EARLY TERTIARY; SYSTEMATICS; CERATOMORPH; OSTEOLOGY; EVOLUTION; EQUIDS AB We describe skulls of the Wasatchian perissodactyl Homogalax and the Bridgerian-Uintan perissodactyl Isectolophus from North America for the first time. These skulls provide information on cranial evolution in tapiromorph perissodactyls as well as on primitive character states for Perissodactyla as a whole. They confirm the retention of a primitive rostrum in these taxa, as Radinsky had previously stated without reference to particular specimens. Characters from skull morphology suggest that Homogalax and Isectolophus should not be included in the same family. C1 Rowan Univ, Dept Biol Sci, Glassboro, NJ 08028 USA. New Mexico Museum Nat Hist, Albuquerque, NM 87104 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Holbrook, LT (reprint author), Rowan Univ, Dept Biol Sci, 201 Mullica Hill Rd, Glassboro, NJ 08028 USA. EM holbrook@rowan.edu NR 34 TC 5 Z9 5 U1 0 U2 3 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 10 PY 2004 VL 24 IS 4 BP 951 EP 956 DI 10.1671/0272-4634(2004)024[0951:SOTEPM]2.0.CO;2 PG 6 WC Paleontology SC Paleontology GA 878QX UT WOS:000225662700017 ER PT J AU Woodman, N AF Woodman, N TI Designation of the type species of Musaraneus Pomel, 1848 (Manunalia : Soricomorpha : Soricidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The genus name Musaraneus often is attributed to Brisson (1762), however, most of Brisson's names are unavailable. Pomel (1848) subsequently made the name Musaraneus available, but did not designate a type species. The 18 species that Pomel listed under Musaraneus currently are distributed among five modern genera, two of which (Cryptotis Pomel, 1848 and Diplomesodon Brandt, 1852) are predated by Musaraneus. Because Cryptotis and Diplomesodon potentially could be considered junior synonyms of Musaraneus, I propose Sorex leucodon Hermann, 1780 (= Crocidura leucodon) as the type species for Musaraneus, thereby establishing Musaraneus as a junior synonym of Crocidura Wagler, 1832. C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. NR 33 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 266 EP 270 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200004 ER PT J AU Malabarba, LR Lima, FCT Weitzman, SH AF Malabarba, LR Lima, FCT Weitzman, SH TI A new species of Kolpotocheirodon (Teleostei : Characidae : Cheirodontinae : Compsurini) from Bahia, northeastern Brazil, with a new diagnosis of the genus SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID FISHES TELEOSTEI; CAUDAL-FIN AB Kolpotocheirodon figueiredoi, a new species of the characid subfamily Cheirodontinae, tribe Compsurini, is described from the upper rio Paraguacu basin, Bahia, Brazil. A new diagnosis for the genus is proposed, based mostly on scanning electron microscope (SEM) analyses of the caudal organ of the new species and that of the single previously known species, Kolpotocheirodon theloura. The genus is diagnosed now in part by the presence of a previously undescribed, sexually dimorphic and apparently glandular, structure found in the lower caudal-fin lobe of males. The basal relative position of Kolpotocheirodon within the Compsurini, in which all species are inseminating, is further supported by the presence of aquasperm in both species rather than the apomorphic elongate sperm nuclei present in the remaining members of the tribe. C1 PUCRS, Museu Ciencias & Tecnol, BR-90619900 Porto Alegre, RS, Brazil. Univ Fed Rio Grande Sul, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil. USP, Museu Zool, BR-04299970 Sao Paulo, Brazil. Smithsonian Inst, Div Fishes, Dept Syst Biol, MRC 0159, Washington, DC 20013 USA. RP Weitzman, SH (reprint author), PUCRS, Museu Ciencias & Tecnol, Av Ipiranga 6681, BR-90619900 Porto Alegre, RS, Brazil. EM malabarb@pucrs.br; fctlima@usp.br; weitzman.stan@nmnh.si.edu RI Malabarba, Luiz/I-3225-2012; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 11 TC 17 Z9 18 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 317 EP 329 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200008 ER PT J AU Castro, RMC Vari, RP AF Castro, RMC Vari, RP TI Astyanax biotae, a new species of stream fish from the Rio Paranapanema basin, upper Rio Parana system, southeastern Brazil (Ostariophysi : Characiformes : Characidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Astyanax biotae, a new species of characid, is described from a first-order stream in the Rio Paranapanema basin, upper Rio Parand system, in the interior of the state of Parand, southeastern Brazil. The species differs from its congeners in that region in a combination of morphometric and pigmentary features. C1 Univ Sao Paulo, Lab Ictiol Ribeirao Preto, Fac Filosofia Ciencias & Letras Ribeirao Preto, Dept Biol, BR-14040901 Ribeirao Preto, SP, Brazil. Smithsonian Inst, Museum Natl Hist Nat, Div Fishes, Vertebrate Zool Sect, Washington, DC 20560 USA. RP Castro, RMC (reprint author), Univ Sao Paulo, Lab Ictiol Ribeirao Preto, Fac Filosofia Ciencias & Letras Ribeirao Preto, Dept Biol, Ave Bandeirantes 3900, BR-14040901 Ribeirao Preto, SP, Brazil. EM rmcastro@ffclrp.usp.br; vari.richard@nmnh.si.edu NR 27 TC 8 Z9 9 U1 1 U2 5 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 330 EP 338 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200009 ER PT J AU Benine, RC Pelicao, GZ Vari, RP AF Benine, RC Pelicao, GZ Vari, RP TI Tetragonopterus lemniscatus (Characiformes : Characidae), a new species from the Corantijn River basin in Suriname SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Tetragonopterus lemniscatus, a new species of characid characiform, is described from the Corantijn River basin in western Suriname. The species is readily distinguished from its congeners (T argenteus, T chalceus) by the presence of dark, longitudinal stripes positioned between adjacent scale rows of the lateral surface of the body. C1 Univ Sao Paulo, Dept Biol, Lab Ictiol Ribeirao Preto, BR-14040901 Ribeirao Preto, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. RP Benine, RC (reprint author), Univ Sao Paulo, Dept Biol, Lab Ictiol Ribeirao Preto, Av Bandeirantes,3900, BR-14040901 Ribeirao Preto, Brazil. EM rbenine@hotmail.com; gzpd@usp.br; vari.richard@nmnh.si.edu RI Benine, Ricardo/B-2354-2013 NR 10 TC 5 Z9 7 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 339 EP 345 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200010 ER PT J AU Kornicker, LS Rudjakov, JA AF Kornicker, LS Rudjakov, JA TI Two new species of seven-spined Bathyconchoecia from the North Atlantic and Indian oceans (Crustacea : Ostracoda : Halocypridae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of halocyprid ostracode Bathyconchoecia omega from abyssal depths of the North Atlantic Ocean, off Newfoundland, Canada, is described and illustrated, and a new species Bathyconchoecia georgei is proposed for a specimen from the Indian Ocean previously referred to Bathyconchoecia deeveyae Kornicker, 1969. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20013 USA. Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20013 USA. EM kornicker.louis@nmnh.si.edu; rudyakov@fas.harvard.edu NR 8 TC 2 Z9 2 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 398 EP 407 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200016 ER PT J AU Robinson, H Moore, AJ AF Robinson, H Moore, AJ TI New species and new combinations in Rhysolepis (Heliantheae : Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A narrow circumscription of the genus Viguiera Kunth results in transfer of 58 species of Helianthinae with glabrous stamen filaments, exappendiculate style appendages, and a persistent pappus into Rhysolepis S.F.Blake. Rhysolepis dillonorum from Peru, R. emaciata. from Bolivia, and R. goyasensis, R. hatschbachii, R. laxicymosa, R. santacatarinensis, and R. subtruncata, from Brazil are new species. Viguiera pazensis and V. procumbens are placed in synonymy under Rhysolepis helianthoides, and V. misionensis is combined with R. pilosa. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, MRC 166, Washington, DC 20013 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Robinson, H (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, MRC 166, POB 166, Washington, DC 20013 USA. NR 13 TC 3 Z9 7 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 7 PY 2004 VL 117 IS 3 BP 423 EP 446 PG 24 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 895RH UT WOS:000226880200018 ER PT J AU Cane, F Bear, D Phillips, DF Rosen, MS Smallwood, CL Stoner, RE Walsworth, RL Kostelecky, VA AF Cane, F Bear, D Phillips, DF Rosen, MS Smallwood, CL Stoner, RE Walsworth, RL Kostelecky, VA TI Bound on Lorentz and CPT violating boost effects for the neutron SO PHYSICAL REVIEW LETTERS LA English DT Article ID NOBLE-GAS MASER; HIGHER-DIMENSIONAL THEORIES; TESTS; STRINGS; INVARIANCE; RELATIVITY; ANISOTROPY; PARTICLES; SYMMETRY; ELECTRON AB A search for an annual variation of a daily sidereal modulation of the frequency difference between colocated Xe-129 and He-3 Zeeman masers sets a stringent limit on boost-dependent Lorentz and CPT violation involving the neutron, consistent with no effect at the level of 150 nHz. In the framework of the general standard-model extension, the present result provides the first clean test for the fermion sector of the symmetry of spacetime under boost transformations at a level of 10(-27) GeV. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Phys, Bloomington, IN 47405 USA. RP Cane, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Smallwood, Christopher/D-4925-2011; OI Smallwood, Christopher/0000-0002-4103-8748; Stoner, Richard/0000-0001-7949-6747 NR 53 TC 92 Z9 92 U1 0 U2 0 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 DEC 3 PY 2004 VL 93 IS 23 AR 230801 DI 10.1103/PhysRevLett.93.230801 PG 4 WC Physics, Multidisciplinary SC Physics GA 876OY UT WOS:000225508000011 PM 15601138 ER PT J AU Eisaman, MD Childress, L Andre, A Massou, F Zibrov, AS Lukin, MD AF Eisaman, MD Childress, L Andre, A Massou, F Zibrov, AS Lukin, MD TI Shaping quantum pulses of light via coherent atomic memory SO PHYSICAL REVIEW LETTERS LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; PHOTON STATES; ENSEMBLES; COMMUNICATION; GENERATION; STORAGE; DEVICE; NOISE AB We describe proof-of-principle experiments demonstrating a novel approach for generating pulses of light with controllable photon numbers, propagation direction, timing, and pulse shapes. The approach is based on preparation of an atomic ensemble in a state with a desired number of atomic spin excitations, which is later converted into a photon pulse. Spatiotemporal control over the pulses is obtained by exploiting long-lived coherent memory for photon states and Electromagnetically Induced Transparency in an optically dense atomic medium. Using photon counting experiments, we observe Electromagnetically Induced Transparency based generation and shaping of few-photon sub-Poissonian light pulses. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. PN Lebedev Phys Inst, Moscow 117924, Russia. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Eisaman, Matthew/E-8006-2011; Childress, Lilian/H-1359-2012; Zibrov, Alexander/G-7419-2014 OI Eisaman, Matthew/0000-0002-3814-6430; Childress, Lilian/0000-0002-0507-6392; NR 24 TC 98 Z9 99 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 3 PY 2004 VL 93 IS 23 AR 233602 DI 10.1103/PhysRevLett.93.233602 PG 4 WC Physics, Multidisciplinary SC Physics GA 876OY UT WOS:000225508000031 PM 15601158 ER PT J AU Ehret, C Keita, SOY Newman, P AF Ehret, C Keita, SOY Newman, P TI The origins of Afroasiatic SO SCIENCE LA English DT Letter ID HAPLOTYPES C1 Univ Calif Los Angeles, Dept Hist, Los Angeles, CA 90095 USA. Howard Univ, Howard Univ Hosp, Natl Human Genome Ctr, Washington, DC 20060 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Washington, DC 20560 USA. Indiana Univ, Dept Linguist, Bloomington, IN 47405 USA. RP Ehret, C (reprint author), Univ Calif Los Angeles, Dept Hist, Los Angeles, CA 90095 USA. NR 15 TC 20 Z9 20 U1 2 U2 3 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 3 PY 2004 VL 306 IS 5702 BP 1680 EP 1681 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 878FA UT WOS:000225630800017 PM 15576591 ER PT J AU Squyres, SW Arvidson, RE Bell, JF Bruckner, J Cabrol, NA Calvin, W Carr, MH Christensen, PR Clark, BC Crumpter, L Des Marais, DJ d'Uston, C Economou, T Farmer, J Farrand, W Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Haskin, L Herkenhoff, KE Hviid, S Johnson, J Klingelhofer, G Knoll, AH Landis, G 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 Sims, M Smith, M Smith, P Soderblom, LA Sutlivan, R Wanke, H Wdowiak, T Wolff, M Yen, A AF Squyres, SW Arvidson, RE Bell, JF Bruckner, J Cabrol, NA Calvin, W Carr, MH Christensen, PR Clark, BC Crumpter, L Des Marais, DJ d'Uston, C Economou, T Farmer, J Farrand, W Folkner, W Golombek, M Gorevan, S Grant, JA Greeley, R Grotzinger, J Haskin, L Herkenhoff, KE Hviid, S Johnson, J Klingelhofer, G Knoll, AH Landis, G 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 Sims, M Smith, M Smith, P Soderblom, LA Sutlivan, R Wanke, H Wdowiak, T Wolff, M Yen, A TI The Opportunity Rover's Athena science investigation at Meridiani Planum, Mars SO SCIENCE LA English DT Article ID X-RAY SPECTROMETER; EXPLORATION ROVERS; MOSSBAUER SPECTROMETER; MICROSCOPIC IMAGER; TERRA-MERIDIANI; MINI-TES; ART.; HEMATITE; MISSION; CRATER AB The Mars Exploration Rover Opportunity has investigated the landing site in Eagle crater and the nearby plains within Meridiani Planum. The soils consist of fine-grained basaltic sand and a surface tag of hematite-rich spherules, spherule fragments, and other granules. Wind ripples are common. Underlying the thin soil layer, and exposed within small impact craters and troughs, are flat-lying sedimentary rocks. These rocks are finely laminated, are rich in sulfur, and contain abundant sulfate salts. Small-scale cross-lamination in some locations provides evidence for deposition in flowing liquid water. We interpret the rocks to be a mixture of chemical and silicictastic sediments formed by episodic inundation by shallow surface water, followed by evaporation, exposure, and desiccation. Hematite-rich spherules are embedded in the rock and eroding from them. We interpret these spherules to be concretions formed by postdepositional diagenesis, again involving liquid water. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Max Planck Inst Chem, D-55128 Mainz, Germany. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Univ Nevada, Dept Geol Sci, 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. Ctr Etud Spatiale Rayonnements, Toulouse, France. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Honeybee Robot, New York, NY 10012 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Max Planck Inst Aeron, Katlenburg Lindau, Germany. Johannes Gutenberg Univ Mainz, 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, Orsted Lab, DK-2100 Copenhagen, Denmark. Malin Space Sci Syst, San Diego, CA 92191 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 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 30907 USA. RP Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI Lemmon, Mark/E-9983-2010; Moersch, Jeffrey/F-7189-2010; Smith, Michael/C-8875-2012; Madsen, Morten/D-2082-2011 OI Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111 NR 34 TC 315 Z9 321 U1 13 U2 55 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD DEC 3 PY 2004 VL 306 IS 5702 BP 1698 EP 1703 DI 10.1126/science.1106171 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 878FA UT WOS:000225630800034 PM 15576602 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Stellar encounters as the origin of distant Solar System objects in highly eccentric orbits SO NATURE LA English DT Article ID KUIPER-BELT OBJECTS; SIZE DISTRIBUTION; ANALOG; BODIES; PLANET; CLOUD; DISKS; DUST; SUN AB The Kuiper belt(1) extends from the orbit of Neptune at 30 AU to an abrupt outer edge about 50 AU from the Sun(2). Beyond the edge is a sparse population of objects with large orbital eccentricities(3,4). Neptune shapes the dynamics of most Kuiper belt objects, but the recently discovered planet 2003 VB12 (Sedna(5)) has an eccentric orbit with a perihelion distance of 70 AU, far beyond Neptune's gravitational influence(6-8). Although influences from passing stars could have created the Kuiper belt's outer edge and could have scattered objects into large, eccentric orbits(9,10), no model currently explains the properties of Sedna. Here we show that a passing star probably scattered Sedna from the Kuiper belt into its observed orbit. The likelihood that a planet at 60-80 AU can be scattered into Sedna's orbit is about 50 per cent; this estimate depends critically on the geometry of the fly-by. Even more interesting is the similar to10 per cent chance that Sedna was captured from the outer disk of the passing star. Most captures have very high inclination orbits; detection of such objects would confirm the presence of extrasolar planets in our own Solar System. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, JFB 201, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 30 TC 73 Z9 74 U1 0 U2 2 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 2 PY 2004 VL 432 IS 7017 BP 598 EP 602 DI 10.1038/nature03136 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 875PL UT WOS:000225433200039 PM 15577903 ER PT J AU Iriarte, J Holst, I Marozzi, O Listopad, C Alonso, E Rinderknecht, A Montana, J AF Iriarte, J Holst, I Marozzi, O Listopad, C Alonso, E Rinderknecht, A Montana, J TI Evidence for cultivar adoption and emerging complexity during the mid-Holocene in the La Plata basin SO NATURE LA English DT Article ID IDENTIFYING MAIZE; PHYTOLITHS; BRAZIL; PERU AB Multidisciplinary investigations at the Los Ajos archaeological mound complex in the wetlands of southeastern Uruguay challenge the traditional view that the La Plata basin was inhabited by simple groups of hunters and gatherers for much of the pre-Hispanic era(1-4). Here we report new archaeological, palaeoecological and botanical data indicating that during an increasingly drier mid-Holocene, at around 4,190 radiocarbon (C-14) years before present (BP), Los Ajos became a permanent circular plaza village, and its inhabitants adopted the earliest cultivars known in southern South America. The architectural plan of Los Ajos during the following Ceramic Mound Period ( around 3,000-500 C-14 yr B P) is similar to, but earlier than, settlement patterns demonstrated in Amazonia(5-10), revealing a new and independent architectural tradition for South America. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. Fac Humanidades & Ciencias Educ, Dept Antropol, Montevideo 1200, Uruguay. Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. Univ Republica, Fac Quim, Dept Bot, Montevideo, Uruguay. Museo Nacl Hist Nat, Montevideo, Uruguay. Museo Nacl Antropol, Montevideo, Uruguay. Univ Republica, Fac Agron, Montevideo 12900, Uruguay. RP Iriarte, J (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 2072, Balboa, Panama. EM iriartej@ancon.si.edu RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 NR 30 TC 70 Z9 72 U1 0 U2 10 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 2 PY 2004 VL 432 IS 7017 BP 614 EP 617 DI 10.1038/nature02983 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 875PL UT WOS:000225433200044 PM 15577908 ER PT J AU Stine, JK AF Stine, JK TI Industrializing organisms: Introducing evolutionary history. SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD DEC PY 2004 VL 109 IS 5 BP 1533 EP 1534 DI 10.1086/530941 PG 2 WC History SC History GA 890UG UT WOS:000226535800012 ER PT J AU Winn, JN Lovell, JEJ Bignall, H Gaensler, BM Getts, TJ Kedziora-Chudczer, L Ojha, R Reynolds, JE Tingay, SJ Tzioumis, T Wieringa, M AF Winn, JN Lovell, JEJ Bignall, H Gaensler, BM Getts, TJ Kedziora-Chudczer, L Ojha, R Reynolds, JE Tingay, SJ Tzioumis, T Wieringa, M TI The radio variability of the gravitational lens PMN J1838-3427 SO ASTRONOMICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (PMN J1838-3427); radio continuum : ISM; scattering; techniques : interferometric ID GIGAHERTZ-PEAKED-SPECTRUM; TIME DELAYS; QUASAR; SCINTILLATION; PARAMETER; MODELS; GALAXY; GHZ AB We present the results of a radio variability study of the gravitational lens PMN J1838 - 3427. Our motivation was to determine the Hubble constant by measuring the time delay between variations of the two quasar images. We monitored the system for 4 months ( approximately 5 times longer than the expected delay) using the Australia Telescope Compact Array at 9 GHz. Although both images were variable on a timescale of a few days, no correlated intrinsic variability could be identified, and therefore no time delay could be measured. Notably, the fractional variation of the fainter image (8%) was greater than that of the brighter image (4%), whereas lensed images of a point source would have the same fractional variation. This effect can be explained, at least in part, as the refractive scintillation of both images due to the turbulent interstellar medium of the Galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. VLBI Europe, Joint Inst, NL-7990 AA Dwingeloo, Netherlands. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jwinn@cfa.harvard.edu; jim.lovell@csiro.au; bignall@jive.nl; bgaensler@cfa.harvard.edu; tracy@marquarding.com; lucyna.kedziora-chudczer@csiro.au; rojha@atnf.csiro.au; john.reynolds@csiro.au; stingay@astro.swin.edu.au; tasso.tzioumis@csiro.au; mark.wieringa@csiro.au RI Gaensler, Bryan/F-8655-2010; Tingay, Steven/B-5271-2013; Bignall, Hayley/B-2867-2013; OI Bignall, Hayley/0000-0001-6247-3071; Gaensler, Bryan/0000-0002-3382-9558 NR 34 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2004 VL 128 IS 6 BP 2696 EP 2703 DI 10.1086/425881 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875JX UT WOS:000225417500007 ER PT J AU Doane, NE Sanders, WT Wilcots, EM Juda, M AF Doane, NE Sanders, WT Wilcots, EM Juda, M TI The origin and distribution of diffuse hot gas in the spiral galaxy NGC 3184 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 3184); galaxies : ISM; X-rays : diffuse background; X-rays : galaxies; X-rays : ISM ID X-RAY-EMISSION; CHANDRA OBSERVATIONS; SUPERBUBBLES; EVOLUTION; STARBURST; BUBBLES; MODELS; CLOUD; M101 AB Deep Chandra exposures reveal the presence of diffuse X-ray emission with a luminosity of 1.3 x 10(39) ergs s(-1) from the spiral galaxy NGC 3184. This appears to be truly diffuse thermal emission distinct from the low-luminosity emission from low-mass X-ray binaries (LMXBs). While the unresolved emission from older LMXBs is more uniformly distributed across the galaxy, the diffuse X-ray emission is concentrated in areas of younger stellar populations and star-forming regions. The surface brightness of the diffuse emission over the spiral arms is 5 times greater than in off-arm regions, and 8 times brighter in H II regions than in non - H II regions. Spectral fits to the diffuse thermal emission are consistent with a low-temperature component, T similar to 1.5 x 10(6) K, plus a higher temperature component, T similar to 5 x 10(6) K. C1 Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Doane, NE (reprint author), Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA. EM doane@astro.wisc.edu; ewilcots@astro.wisc.edu OI Juda, Michael/0000-0002-4375-9688 NR 36 TC 11 Z9 11 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 2004 VL 128 IS 6 BP 2712 EP 2723 DI 10.1086/425627 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875JX UT WOS:000225417500009 ER PT J AU Kong, AKH Sjouwerman, LO Williams, BF AF Kong, AKH Sjouwerman, LO Williams, BF TI X-ray-optical-radio observations of a resolved supernova remnant in NGC 6822 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 6822); supernova remnants; X-rays : ISM ID LARGE-MAGELLANIC-CLOUD; NEARBY GALAXIES; ROSAT HRI; CATALOG; REGIONS; SPECTROSCOPY; DISCOVERY; EMISSION; CHANDRA; ATLAS AB The supernova remnant (SNR) Ho 12, in the center of the dwarf irregular galaxy NGC 6822, was previously observed at X-ray, optical, and radio wavelengths. By using archival Chandra and ground-based optical data, we found that the SNR is spatially resolved in X-rays and optical. In addition, we obtained a similar to5" resolution radio image of the SNR. These observations provide the highest spatial resolution imaging of an X-ray -optical-radio SNR in that galaxy to date. The multiwavelength morphology, X-ray spectrum and variability, and narrowband optical imagings are consistent with an SNR. The SNR is a shell-shaped object with a diameter of about 10" (24 pc). The morphology of the SNR is consistent across the wavelengths, while the Chandra spectrum can be well fitted with a nonequilibrium ionization model with an electron temperature of 2.8 keV and a 0.3 - 7 keV luminosity of 1.6 x 10(37) ergs s(-1). The age of the SNR is estimated to be 1700 - 5800 yr. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akong@cfa.harvard.edu NR 41 TC 11 Z9 11 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 2004 VL 128 IS 6 BP 2783 EP 2788 DI 10.1086/425527 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875JX UT WOS:000225417500015 ER PT J AU Balog, Z Kenyon, SJ Lada, EA Barsony, M Vinko, J Gaspar, A AF Balog, Z Kenyon, SJ Lada, EA Barsony, M Vinko, J Gaspar, A TI A near-infrared (JHK) survey of the vicinity of the HII region NGC 7538: Evidence for a young embedded cluster SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 7538); stars : formation; stars : luminosity function, mass function; stars : pre-main-sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE TRACKS; H-II REGIONS; IMAGING SURVEY; MILKY-WAY; CIRCUMSTELLAR DISKS; MASS FUNCTION; DARK CLOUD AB We describe the results of two near-infrared (K-band) imaging surveys and a three-color (JHK) survey of the vicinity of NGC 7538. The limiting magnitudes are Ksimilar or equal to16.5 and 17.5 mag for the K-band surveys and Ksimilar or equal to15 mag for the JHK survey. We identify more than 2000 and 9000 near-infrared (NIR) sources on the images of the two K-band surveys and 786 NIR sources in the JHK survey. From color-color diagrams, we derive a reddening law for background stars and identify 238 stars with NIR excesses. Contour maps indicate a high-density peak coincident with a concentration of stars with NIR excesses. We identify this peak as a young embedded cluster and confirm this result with the K-band luminosity function (KLF), color histograms, and color-magnitude diagrams. The center of the cluster is at R.A.=23(h)13(m)39.(s)34, decl.=61degrees29'18"9. The cluster radius is similar to3', similar to2.5 pc for an adopted distance dsimilar or equal to2.8 kpc. For d=2.8 kpc and reddening E(J-K)=0.55 mag, the slope of the logarithmic KLF of the cluster, ssimilar to0.32+/-0.03, agrees well with previous results for L1630 (s=0.34) and M17 (s=0.26) found by C. Lada, E. Lada, and coworkers. C1 Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Space Sci Inst, Boulder, CO 80301 USA. Univ Szeged, Dept Opt & Quantum Elect, H-6701 Szeged, Hungary. RP Balog, Z (reprint author), Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. EM balogz@titan.physx.u-szeged.hu; skenyon@cfa.harvard.edu OI Vinko, Jozsef/0000-0001-8764-7832; Kenyon, Scott/0000-0003-0214-609X NR 60 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2004 VL 128 IS 6 BP 2942 EP 2953 DI 10.1086/425548 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875JX UT WOS:000225417500028 ER PT J AU Czerny, B Rozanska, A Kuraszkiewicz, J AF Czerny, B Rozanska, A Kuraszkiewicz, J TI Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; galaxies : active; galaxies : Seyfert; X-rays : galaxies; quasars : emission lines ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; GEOMETRICALLY THIN DISKS; EMISSION-LINE; X-RAY; SPECTRAL ATLAS; QUASARS; VARIABILITY; NGC-4579; MODEL AB We analyze the consequences of the hypothesis that the formation of the Broad Line Region is intrinsically connected to the existence of the cold accretion disk. We assume that the Broad Line Region radius is reliably estimated by the formula of Kaspi et al. (2000, ApJ, 533, 631). We consider three models of the disappearance of the inner disk that limit the existence of the Broad Line Region: (i) the classical ADAF approach, i.e. the inner hot flow develops whenever it can exist; (ii) the disk evaporation model of Meyer & Meyer-Hofmeister (2002, AA, 392, L5); (iii) the generalized disk evaporation model of Rozanska & Czerny (2000b, A&A, 360, 1170). For each of the models, we determine the minimum value of the Eddington ratio and the maximum value of the broad line widths as functions of the viscosity parameter a and the magnetic field parameter beta. We compare the predicted parameter space with observations of several AGN. Weak dependence of the maximum value of the FWHM and minimum value of the Eddington ratio on the black hole mass in our sample is noticeable. It seems to favor the description of the cold disk/hot inner flow transition as in the classical ADAF approach rather than with the model of disk evaporation due to conduction between the disk and accreting corona. C1 Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Czerny, B (reprint author), Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM bcz@camk.edu.pl RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 66 TC 41 Z9 41 U1 0 U2 0 PU E D P SCIENCES 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 2004 VL 428 IS 1 BP 39 EP U22 DI 10.1051/0004-6361:20040487 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 874EY UT WOS:000225334900007 ER PT J AU Sollerman, J Lindahl, J Kozma, C Challis, P Filippenko, AV Fransson, C Garnavich, PM Leibundgut, B Li, W Lundqvist, P Milne, P Spyromilio, J Kirshner, RP AF Sollerman, J Lindahl, J Kozma, C Challis, P Filippenko, AV Fransson, C Garnavich, PM Leibundgut, B Li, W Lundqvist, P Milne, P Spyromilio, J Kirshner, RP TI The late-time light curve of the type Ia supernova 2000cx SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : supernovae : general; stars : supernovae : individual : SN 2000cx ID ELECTRON-ION RECOMBINATION; LATE SPECTRAL EVOLUTION; STANDARD STARS; SN 1987A; EMISSION; MODELS; NOVAE; NUCLEOSYNTHESIS; IONIZATION; PHOTOMETRY AB We have conducted a systematic and comprehensive monitoring programme of the type Ia supernova 2000cx at late phases using the VLT and HST. The VLT observations cover phases 360 to 480 days past maximum brightness and include photometry in the BVRIJH bands, together with a single epoch in each of U and K-s. While the optical bands decay by about 1.4 mag per 100 days, we find that the near-IR magnitudes stay virtually constant during the observed period. This means that the importance of the near-IR to the bolometric light curve increases with time. The finding is also in agreement with our detailed modeling of a type Ia supernova in the nebular phase. In these models, the increased importance of the near-IR is a temperature effect. We note that this complicates late-time studies where often only the V band is well monitored. In particular, it is not correct to assume that any optical band follows the bolometric light curve at these phases, and any conclusions based on such assumptions, e. g., regarding positron-escape, must be regarded as premature. A very simple model where all positrons are trapped can reasonably well account for the observations. The nickel mass deduced from the positron tail of this light curve is lower than found from the peak brightness, providing an estimate of the fraction of late-time emission that is outside of the observed wavelength range. Our detailed models show the signature of an infrared catastrophe at these epochs, which is not supported by the observations. C1 Stockholm Observ, AlbaNova, Dept Astron, S-10691 Stockholm, Sweden. Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46566 USA. European So Observ, D-85748 Garching, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Stockholm Observ, AlbaNova, Dept Astron, S-10691 Stockholm, Sweden. EM jesper@astro.su.se OI Sollerman, Jesper/0000-0003-1546-6615 NR 56 TC 56 Z9 56 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2004 VL 428 IS 2 BP 555 EP U71 DI 10.1051/0004-6361:20041320 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 874FA UT WOS:000225335100019 ER PT J AU Huelamo, N Fernandez, M Neuhauser, R Wolk, SJ AF Huelamo, N Fernandez, M Neuhauser, R Wolk, SJ TI Rotation periods of Post-T Tauri stars in Lindroos systems SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : pre-main sequence; stars : late-type; stars : rotation; X-rays : stars; stars : binaries : visual ID LOW-MASS STARS; ORION-NEBULA-CLUSTER; MAIN-SEQUENCE STARS; X-RAY-EMISSION; ANGULAR-MOMENTUM EVOLUTION; EARLY-TYPE PRIMARIES; SOLAR-TYPE STARS; YOUNG STARS; STELLAR ROTATION; ACCRETION DISKS AB We present a rotational study of Post-T Tauri stars (PTTSs) in Lindroos systems, defined as binaries with early type primaries on the main-sequence (MS) and late-type secondaries on the pre-main-sequence (PMS) phase. The importance of this study in comparison with previous ones is that the Lindroos sample is not X-ray selected so we avoid a possible bias towards fast rotators. In this preliminary study we have monitored eleven stars in the UBVRI bands during two campaigns of ten consecutive nights each. Eight of the observed PTTSs show periodic modulations in their lightcurves and the derived periods range from 1.9 d to 8.0 d. The comparison of these results with theoretical rotational tracks based on disk-star locking theory shows that star-disk decoupling times of 1-20 Myr could reproduce the rotational properties of the targets, assuming an initial rotation period of similar to8 d and a mass of 1 M-circle dot. We have studied the rotation-activity relations of Lindroos PTTSs and compared them with those found in other groups of PMS and zero-age main-sequence (ZAMS) similar to1 M-circle dot stars. The Lindroos sample displays activity-rotation relations very similar to those found in TTSs. It contains a mixture of very active stars, with L-X/L-bol ratios close to the saturation level of -3, and less active (unsaturated) stars. This could be the result of different star-disk decoupling times. Future monitoring of a larger and unbiased sample of PTTS will be important to confirm the significance of these results. C1 European So Observ, Santiago 19, Chile. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Jena, Inst Astrophys, D-07745 Jena, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huelamo, N (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile. EM nhuelamo@eso.org RI Huelamo, Nuria/C-3042-2017; OI Huelamo, Nuria/0000-0002-2711-8143; Wolk, Scott/0000-0002-0826-9261 NR 68 TC 3 Z9 3 U1 0 U2 0 PU E D P SCIENCES 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 2004 VL 428 IS 3 BP 953 EP 967 DI 10.1051/0004-6361:20034442 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 877UT UT WOS:000225599800021 ER PT J AU Fabbiano, G Baldi, A Pellegrini, S Siemiginowska, A Elvis, M Zezas, A McDowell, J AF Fabbiano, G Baldi, A Pellegrini, S Siemiginowska, A Elvis, M Zezas, A McDowell, J TI Chandra observations of the quiescent nuclear black hole of NGC 821: Evidence of nuclear activity? SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (NGC 821); galaxies : nuclei; X-rays : galaxies ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; X-RAY JET; ELLIPTIC GALAXIES; NEARBY GALAXIES; GALACTIC NUCLEI; COOLING FLOWS; M87 JET; NGC-1316 FORNAX; EMISSION AB We report the results of the Chandra ACIS-S observations of the elliptical galaxy NGC 821, which harbors a supermassive nuclear black hole (3.5 x 10(7) M(circle dot)) but does not show signs of active galactic nucleus activity. A small, 8."5 long (similar to1 kpc at the galaxy's distance of 23 Mpc), possibly S-shaped, jetlike feature centered on the nucleus is detected in the 38 ks ACIS-S integrated exposure of this region. The luminosity of this feature is L(X) similar to 2.6 x 10(39) ergs s(-1) (0.3-10 keV), and its spectrum is hard (described by a power law of Gamma = 1.8(-0.6)(+0.7) or by thermal emission with kT > 2 keV). We discuss two possibilities for the origin of this feature: (1) a low-luminosity X-ray jet, or (2) a hot shocked gas. In either case, it is a clear indication of nuclear activity, detectable only in the X-ray band. Steady spherical accretion of the mass losses from the central stellar cusp within the accretion radius, when coupled with a high radiative efficiency, already provides a power source exceeding the observed radiative losses from the nuclear region. A third possibility, that this feature may arise from a fortuitous distribution of luminous X-ray binaries in NGC 821, is also discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu; abaldi@cfa.harvard.edu; silvia.pellegrini@unibo.it; aneta@cfa.harvard.edu; elvis@cfa.harvard.edu; azezas@cfa.harvard.edu; jcm@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 68 TC 24 Z9 24 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 DEC 1 PY 2004 VL 616 IS 2 BP 730 EP 737 DI 10.1086/424919 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100006 ER PT J AU Rodriguez-Rico, CA Viallefond, F Zhao, JH Goss, WM Anantharamaiah, KR AF Rodriguez-Rico, CA Viallefond, F Zhao, JH Goss, WM Anantharamaiah, KR TI Very large array H92 alpha and H53 alpha radio recombination line observations of M82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M82); galaxies : ISM; galaxies : starburst; HII regions; radio lines : galaxies ID STARBURST GALAXY M82; H-II REGIONS; SUPERNOVA-REMNANTS; BARRED GALAXY; NUCLEUS; RESOLUTION; CONTINUUM; EMISSION; NGC-253; M-82 AB We present high angular resolution (0."6) observations made with the Very Large Array of the radio continuum at 8.3 and 43 GHz, as well as H92alpha and H53alpha radio recombination lines from the nearby (similar to3 Mpc) starburst galaxy M82. In the continuum we identify 58 sources at 8.3 GHz, of which 19 have no counterparts in catalogs published at other frequencies. At 43 GHz we identify 18 sources, unresolved at 0."6 resolution, of which five were unknown previously. The spatial distribution of the H92alpha line is inhomogeneous; we identify 27 features; about half of them are associated with continuum emission sources. Their sizes are typically in the range 2-10 pc. Although observed with poorer signal-to-noise ratio, the H53alpha line is detected. The line and continuum emission are modeled using a collection of H II regions at different distances from the nucleus. The observations can be interpreted assuming a single-density component, but equally well with two components if constraints originating from previous high-resolution continuum observations are used. The high-density component has a density of similar to4 x 10(4) cm(-3). However, the bulk of the ionization is in regions with densities that are typically a factor of 10 lower. The gas kinematics, using the H92alpha line, confirms the presence of steep velocity gradient (26 km s(-1) arcsec(-1)) in the nuclear region, as previously reported, in particular from observations of the [Ne II] line at 12 mum. This gradient has about the same amplitude on both sides of the nucleus. Since this steep gradient is observed not only on the major axis but also at large distances along a band at P. A. similar to150degrees, the interpretation in terms of x(2) orbits elongated along the minor axis of the bar, which would be observed at an angle close to the inclination of the main disk, seems inadequate. The observed kinematics cannot be modeled using a simple model that consists of a set of circular orbits observed at different tilt angles. Ad hoc radial motions must be introduced to reproduce the pattern of the velocity field. Different families of orbits are indicated since we detect a signature in the kinematics at the transition between the two plateaus observed in the NIR light distribution. These H92alpha data also reveal the base of the outflow where the injection toward the halo on the northern side occurs. The outflow has a major effect on the observed kinematics, present even in the disk at distances close to the nucleus. The kinematic pattern suggests a connection between the gas flowing in the plane of M82 toward the center; this behavior most likely is due to the presence of a bar and the outflow out of the plane. C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. Observ Paris, LERMA, F-75014 Paris, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Raman Res Inst, Bangalore 560080, Karnataka, India. RP Rodriguez-Rico, CA (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA. EM crodrigu@nrao.edu; fviallef@maat.obspm.fr; jzhao@cfa.harvard.edu; mgoss@nrao.edu RI Anantharamaiah , K. R./E-5369-2012; M, Manjunath/N-4000-2014 OI M, Manjunath/0000-0001-8710-0730 NR 39 TC 33 Z9 33 U1 0 U2 1 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 1 PY 2004 VL 616 IS 2 BP 783 EP 803 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100011 ER PT J AU Kim, S Walsh, W Xiao, KC AF Kim, S Walsh, W Xiao, KC TI Antarctic Submillimeter Telescope and Remote Observatory observations of Co-12 J = 4 -> 3 emission from the N44 complex in the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; ISM : atoms; ISM : general; ISM : molecules; Magellanic Clouds; radio lines : galaxies ID PHOTODISSOCIATION REGIONS; MOLECULAR ABUNDANCES; INTERSTELLAR COMPLEX; APERTURE SYNTHESIS; HYDROGEN GAS; CO SURVEY; X-RAYS; LMC; SUPERBUBBLES; ASSOCIATIONS AB We present Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) observations of (CO)-C-12 J = 4 --> 3 and [C I] emission in the N44 H II complex in the Large Magellanic Cloud. We detected strong (CO)-C-12 J = 4 ! 3 emission toward the H II region known as N44BC, which is located on the rim of an expanding giant shell in the N44 region. Analysis with a photodissociation region model showed that the (CO)-C-12 J = 4 --> 3 emitting cloud is very dense, with n(0) approximate to 10(5) cm(-3). We also note that there is a high-velocity component associated with the (CO)-C-12 J = 4 --> 3 emission. This probably originates from molecular material accelerated as a result of the motion induced by the expanding giant shell surrounding LH 47 in the N44 complex. We found that the kinetic energy of this high-velocity gas observed in the (CO)-C-12 J = 4 --> 3 emission toward the rim of the expanding H II shell is at least a factor of 4 higher than that derived for the H I and H II gas in this region. C1 Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, S (reprint author), Sejong Univ, Dept Astron & Space Sci, KunJa Dong 98, Seoul 143747, South Korea. EM skim@arcsec.sejong.ac.kr NR 45 TC 10 Z9 10 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 2004 VL 616 IS 2 BP 865 EP 871 DI 10.1086/425120 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100016 ER PT J AU Reid, MJ Brunthaler, A AF Reid, MJ Brunthaler, A TI The proper motion of Sagittarius A*. II. The mass of Sagittarius A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; black hole physics; Galaxy : center; Galaxy : fundamental parameters; Galaxy : structure ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; IONIZED-GAS; 86 GHZ; POSITION; GALAXY; DYNAMICS; CLUSTER; RADIO; STARS AB We report measurements with the Very Long Baseline Array (VLBA) of the position of Sgr A* with respect to two extragalactic radio sources over a period of 8 yr. The apparent proper motion of Sgr A* relative to J1745-283 is 6.379 +/- 0.024 mas yr(-1) along a position angle of 209.degrees60 +/- 0.degrees18, almost entirely in the plane of the Galaxy. The effects of the orbit of the Sun around the Galactic center can account for this motion, and the residual proper motion of Sgr A* perpendicular to the plane of the Galaxy is -0.4 +/- 0.9 km s(-1). A maximum likelihood analysis of the motion expected for a massive object within the observed Galactic center stellar cluster indicates that Sgr A* contains more than about 10% of the approximate to4 x 10(6) M-circle dot deduced from stellar orbits. The intrinsic size of Sgr A*, as measured by several investigators, is less than 1 AU, and the implied mass density of similar to10(22) M-circle dot pc(-3) is within about 3 orders of magnitude of a comparable supermassive black hole within its Schwarzschild radius. Our observations provide the first direct evidence that a compact radiative source at the center of a galaxy contains of order 10(6) M-circle dot and provides overwhelming evidence that it is in the form of a supermassive black hole. Finally, the existence of "intermediate-mass" black holes more massive than similar to10(4) M-circle dot between roughly 10(3) and 10(5) AU from Sgr A* is excluded. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mreid@cfa.harvard.edu; brunthaler@jive.nl NR 43 TC 320 Z9 323 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 2004 VL 616 IS 2 BP 872 EP 884 DI 10.1086/424960 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100017 ER PT J AU Chen, Y Su, Y Slane, PO Wang, QD AF Chen, Y Su, Y Slane, PO Wang, QD TI A Chandra ACIS view of the thermal composite supernova remnant 3C 391 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (3C 391, G31.9+0.0); radiation mechanisms : thermal; supernova remnants; X-rays : ISM ID MHZ MASER EMISSION; FORMED DENSE SHELL; X-RAY; MODELING W44; HOT INTERIOR; OH; MORPHOLOGY; CLOUDS; SHOCK; 3C-391 AB We present a 60 ks Chandra ACIS-S observation of the thermal composite supernova remnant 3C 391. The southeast-northwest elongated morphology is similar to that previously found in radio and X-ray studies. This observation unveils a highly clumpy structure of the remnant. Detailed spatially resolved spectral analysis of the small-scale features reveals that the interior gas is generally of normal metal abundance and has approached or basically reached ionization equilibrium. The hydrogen column density increases from southeast to northwest. Three mechanisms, radiative rim, thermal conduction, and cloudlet evaporation, may all play roles in the X-ray appearance of 3C 391 as a "thermal composite" remnant, but there are difficulties with each of them in explaining some physical properties. Comparatively, the cloudlet evaporation model is favored by the main characteristics such as the highly clumpy structure and the uniform temperature and density distribution over most of the remnant. The directly measured postshock temperature also implies a young age, similar to4 x 10(3) yr, for the remnant. The postshock gas pressure derived from the northeast and southwest rims, which harbor maser spots, is consistent with the estimate for the maser regions. An unresolved X-ray source is observed on the northwest border, and its spectrum is best fitted by a power law. C1 Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, Y (reprint author), Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. NR 40 TC 33 Z9 35 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 2004 VL 616 IS 2 BP 885 EP 894 DI 10.1086/425152 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100018 ER PT J AU Luhman, KL AF Luhman, KL TI A survey for low-mass stars and brown dwarfs in the eta Chamaeleontis and epsilon Chamaeleontis young associations SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : emission-line, Be; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID HERBIG AE/BE STARS; FORMING REGION; EVOLUTIONARY MODELS; OPEN CLUSTER; PHOTOMETRY; DISCOVERY; HD-104237; MEMBERS; COLORS; CENSUS AB I present the results of a search for new low-mass stars and brown dwarfs in the eta Cha and epsilon Cha young associations. Within radii of 1.degrees5 and 0.degrees5 surrounding eta Cha and epsilon Cha, respectively, I have constructed color-magnitude diagrams from Deep Near Infrared Survey (DENIS) and Two Micron All Sky Survey (2MASS) photometry and have obtained spectra of the candidate low-mass members therein. The five candidates in eta Cha are classified as four field M dwarfs and one carbon star. No new members are found in this survey, which is complete for M/M-circle dot = 0.015-0.15, according to the evolutionary models of Chabrier and Baraffe. Thus, an extended population of low-mass members is not present in eta Cha out to 4 times the radius of the known membership. Meanwhile, the three candidate members of eta Cha are classified as young stars, and thus likely members of the association, based on Li absorption and gravity-sensitive absorption lines. These new sources have spectral types of M2.25, M3.75, and M5.75, corresponding to masses of 0.45, 0.25, and 0.09 M-circle dot by the models of Chabrier and Baraffe. For one of these stars, intense Halpha emission, forbidden line emission, and strong K-band excess emission suggest the presence of accretion, an outflow, and a disk, respectively. This young star is also much fainter than expected for an association member at its spectral type, which could indicate that it is seen in scattered light. No brown dwarfs are detected in epsilon Cha down to the completeness limit of 0.015 M-circle dot. The absence of brown dwarfs in these associations is statistically consistent with the mass functions measured in star-forming regions, which exhibit only similar to2 and similar to1 brown dwarfs for stellar samples at the sizes of the eta Cha and epsilon Cha associations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu NR 31 TC 32 Z9 32 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 2004 VL 616 IS 2 BP 1033 EP 1041 DI 10.1086/424963 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100027 ER PT J AU Camilo, F Gaensler, BM Gotthelf, EV Halpern, JP Manchester, RN AF Camilo, F Gaensler, BM Gotthelf, EV Halpern, JP Manchester, RN TI Chandra detection of a synchrotron nebula around the Vela-like pulsar J1016-5857 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G284.0-1.8. G284.3-1.8); pulsars : individual (PSR J1016-5857); stars : individual (CXOU J101623.6-585542); supernova remnants ID GAMMA-RAY SOURCES; X-RAY; SUPERNOVA REMNANT; PSR J2229+6114; WIND NEBULAE; DISCOVERY AB We report on a 19 ks observation of the pulsar J1016-5857 with the Chandra X-Ray Observatory. This "Velalike'' pulsar has rotation period 107 ms, characteristic age 21 kyr, and spin-down power 2.6 x 10(36) ergs s(-1). A relatively bright, centrally peaked source of radius approximate to25" around the radio pulsar position has a spectrum that is well fitted by an absorbed power law with photon index 1.32 +/- 0.25. We regard this as a newly identified pulsar wind nebula (PWN) that we designate PWN G284.0-1.8. We do not detect the pulsar as either a point X-ray source or a pulsed source in a 55 ks observation with the Rossi X-Ray Timing Explorer. The isotropic PWN luminosity is 3 x 10(32) ergs s(-1) in the 2-10 keV range, for a distance of 3 kpc that is consistent with the measured neutral hydrogen column density. The unpulsed flux from the pulsar is less than 30% of the measured PWN flux. The brightest component of the PWN, near the pulsar, shows extended emission of size similar to2" that may indicate, by analogy with other young pulsars, the wind termination shock. In the Chandra image we also detect a very faint extended structure approximate to1' x 2' in size that is highly asymmetric about the pulsar position. This structure is a good match in width and position angle to the tip of a "finger'' of radio emission that appears to connect to the nearby supernova remnant G284.3-1.8, but we cannot characterize it further with the available data. There is a variable X-ray point source only 1'5 from the pulsar, which we identify using optical spectroscopy as an accreting binary. C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, 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 Gaensler, Bryan/0000-0002-3382-9558 NR 25 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2004 VL 616 IS 2 BP 1118 EP 1123 DI 10.1086/424924 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100037 ER PT J AU Yoo, JY DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Szymanski, MK Udalski, A Szewczyk, O Kubiak, M Zebrun, K Pietrzynski, G Soszynski, I Wyrzykowski, L AF Yoo, JY DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Szymanski, MK Udalski, A Szewczyk, O Kubiak, M Zebrun, K Pietrzynski, G Soszynski, I Wyrzykowski, L CA muFUN Collaboration OGLE Collaboration TI Constraints on planetary companions in the magnification A=256 microlensing event OGLE-2003-BLG-423 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy : bulge; gravitational lensing; planetary systems; stars : low-mass, brown dwarfs ID GRAVITATIONAL LENSING EXPERIMENT; INITIAL MASS FUNCTION; EXTRASOLAR PLANETS; GALACTIC BULGE; STELLAR; LIMITS; ABUNDANCE; CAMPAIGN; SYSTEMS; SEARCH AB We develop a new method of modeling microlensing events based on a Monte Carlo simulation that incorporates both a Galactic model and the constraints imposed by the observed characteristics of the event. The method provides an unbiased way to analyze the event, especially when parameters are poorly constrained by the observed light curve. We apply this method to search for planetary companions of the lens in OGLE-2003-BLG-423, whose maximum magnification A(max) = 256 +/- 43 (or A(max) = 400 +/- 115 from the light- curve data alone) is the highest among single-lens events ever recorded. The method permits us for the first time to place constraints directly in the planet mass - projected physical separation plane rather than in the mass ratio - Einstein radius plane as was done previously. For example, Jovian-mass companions of main-sequence stars at 2.5 AU are excluded with 80% efficiency. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Dept Astron, Pasadena, CA 91025 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Inst Basic Sci Res, Dept Phys, Chonju 361763, South Korea. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Korea Astron Observ, Taejon 305348, South Korea. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Concepcion, Dept Fis, Concepcion, Chile. RP Yoo, JY (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM jaiyul@astronomy.ohio-state.edu; depoy@astronomy.ohio-state.edu; avishay@astro.caltech.edu; sgaudi@cfa.harvard.edu; gould@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; yiftah@astronomy.ohio-tate.edu; dani@astronomy.ohio-state.edu; eran@astronomy.ohio-state.edu; bgpark@boao.re.kr; pogge@astronomy.ohio-state.edu; msz@astrouw.edu.pl; udalski@astrouw.edu.pl; szewczyk@astrouw.edu.pl; mk@astrouw.edu.pl; zebrun@astrouw.edu.pl; pietrzyn@astrouw.edu; soszynsk@astrouw.edu.pl; lukas@astronomy.ohio-state.edu RI Gaudi, Bernard/I-7732-2012 NR 26 TC 29 Z9 29 U1 0 U2 1 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 1 PY 2004 VL 616 IS 2 BP 1204 EP 1214 DI 10.1086/424988 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KC UT WOS:000225418100045 ER PT J AU Neilsen, J Hickox, RC Vrtilek, SD AF Neilsen, J Hickox, RC Vrtilek, SD TI Phase variation in the pulse profile of SMC X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars : individual (SMC X-1); stars : neutron; X-rays : binaries ID X-RAY PULSARS; SMC X-1; PERIOD; CHANDRA AB We present the results of the timing and spectral analysis of X-ray high-state observations of the high-mass X-ray pulsar SMC X-1 with Chandra, XMM-Newton, and ROSAT, taken between 1991 and 2001. The source has L-x similar to (3-5) x 10(38) ergs s(-1), and the spectra can be modeled as a power law plus blackbody with kT(BB) similar to0.18 and a reprocessed emission radius R-BB similar to 2 x 10(8) cm, assuming a distance of 60 kpc to the source. Energy-resolved pulse profiles show several distinct forms, more than half of which include a second pulse in the soft profile, previously documented only in hard energies. We also detect significant variation in the phase shift between hard and soft pulses, as has recently been reported in Her X-1. We suggest an explanation for the observed characteristics of the soft pulses in terms of precession of the accretion disk. C1 Kenyon Coll, Dept Phys, Gambier, OH 43022 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Neilsen, J (reprint author), Kenyon Coll, Dept Phys, Gambier, OH 43022 USA. EM neilsenj@kenyon.edu; rhickox@cfa.harvard.edu; saku@head.cfa.harvard.edu NR 15 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2004 VL 616 IS 2 BP L135 EP L138 DI 10.1086/426890 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KJ UT WOS:000225418800016 ER PT J AU Shahbaz, T Casares, J Watson, CA Charles, PA Hynes, RI Shih, SC Steeghs, D AF Shahbaz, T Casares, J Watson, CA Charles, PA Hynes, RI Shih, SC Steeghs, D TI The massive neutron star or low-mass black hole in 2S 0921-630 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (V395 Carinae); stars : neutron; X-rays : binaries; X-rays : individual (2S 0921-630) ID X-RAY BINARIES; OPTICAL LIGHT CURVES; NOVA SCORPII 1994; CYGNUS X-2; COMPANION STAR; ACCRETION DISK; GRO J1655-40; 2S 0921-630; MODEL; OSCILLATIONS AB We report on the optical spectroscopy of the eclipsing halo low-mass X-ray binary 2S 0921-630, which reveals the absorption-line radial velocity curve of the K0 III secondary star with a semiamplitude K(2)=92.89+/-3.84 km s(-1), a systemic velocity gamma=34.9+/-3.3 km s(-1), and an orbital period P(orb) of 9.0035+/-0.0029 days (1 sigma). Given the quality of the data, we find no evidence for the effects of X-ray irradiation. Using the previously determined rotational broadening of the mass donor and applying conservative limits on the orbital inclination, we constrain the compact object mass to be 2.0-4.3 M(circle dot) (1 sigma), ruling out a canonical neutron star at the 99% level. Since the nature of the compact object is unclear, this mass range implies that the compact object is either a low-mass black hole with a mass slightly higher than the maximum possible neutron star mass (2.9 M(circle dot)) or a massive neutron star. If the compact object is a black hole, it confirms the prediction of the existence of low-mass black holes, while if the object is a massive neutron star, its high mass severely constrains the equation of state of nuclear matter. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shahbaz, T (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain. EM tsh@ll.iac.es; jcv@ll.iac.es; c.watson@sheffield.ac.uk; pac@soton.ac.uk; rih@astro.as.utexas.edu; icshih@soton.ac.uk; steeghs@cfa.harvard.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 34 TC 23 Z9 23 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 1 PY 2004 VL 616 IS 2 BP L123 EP L126 DI 10.1086/426504 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KJ UT WOS:000225418800013 ER PT J AU Sozzetti, A Yong, D Torres, G Charbonneau, D Latham, DW Prieto, CA Brown, TM Carney, BW Laird, JB AF Sozzetti, A Yong, D Torres, G Charbonneau, D Latham, DW Prieto, CA Brown, TM Carney, BW Laird, JB TI High-resolution spectroscopy of the transiting planet host star TrES-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; stars : abundances; stars : individual (TrES-1) ID EXTRASOLAR GIANT PLANETS; SOLAR-TYPE STARS; CA-II H; EVOLUTIONARY TRACKS; MAGNETIC ACTIVITY; PARENT STARS; TELESCOPE; HD-209458; OGLE-TR-56B; CANDIDATES AB We report on a spectroscopic determination of the stellar parameters and chemical abundances for the parent star of the transiting planet TrES-1. Based on a detailed analysis of iron lines in our Keck and Hobby-Eberly Telescope spectra, we derive T-eff = 5250 +/- 75 K, log g = 4.6 +/- 0.2, and [Fe/H] = 0.00 +/- 0.09. By measuring the Ca II activity indicator and by putting useful upper limits on the Li abundance, we constrain the age of TrES-1 to be 2.5 +/- 1.5 Gyr. By comparing theoretical stellar evolution models with the observational parameters, we obtain M* = 0.89 +/- 0.05 M-. and R-* = 0.83 +/- 0.05 R-.. Our improved estimates of the stellar parameters are utilized in a new analysis of the transit photometry of TrES-1 to derive a mass M-p = (0.76 +/- 0.05) M-J, a radius R-p = 1.04(-0.05)(+0.08) R-J, and an inclination i = 89.5(-1.3)(+0.5) deg. The improved planetary mass and radius estimates provide the grounds for new crucial tests of theoretical models of evolution and evaporation of irradiated extrasolar giant planets. C1 Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. RP Sozzetti, A (reprint author), Univ Pittsburgh, Dept Phys & Astron, 100 Allen Hall,3941 OHara St, Pittsburgh, PA 15260 USA. EM asozzett@cfa.harvard.edu; yong@physics.unc.edu; gtorres@cfa.harvard.edu; dcharbon@cfa.harvard.edu; dlatham@cfa.harvard.edu; callende@hebe.as.utexas.edu; timbrown@hao.ucar.edu; bruce@physics.unc.edu; laird@tycho.bgsu.edu OI Sozzetti, Alessandro/0000-0002-7504-365X; Charbonneau, David/0000-0002-9003-484X NR 38 TC 54 Z9 54 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 2004 VL 616 IS 2 BP L167 EP L170 DI 10.1086/426864 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 875KJ UT WOS:000225418800024 ER PT J AU Szokoly, GP Bergeron, J Hasinger, G Lehmann, I Kewley, L Mainieri, V Nonino, M Rosati, P Giacconi, R Gilli, R Gilmozzi, R Norman, C Romaniello, M Schreier, E Tozzi, P Wang, JX Zheng, W Zirm, A AF Szokoly, GP Bergeron, J Hasinger, G Lehmann, I Kewley, L Mainieri, V Nonino, M Rosati, P Giacconi, R Gilli, R Gilmozzi, R Norman, C Romaniello, M Schreier, E Tozzi, P Wang, JX Zheng, W Zirm, A TI The Chandra Deep Field-South: Optical spectroscopy. I. SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology : observations; galaxies : active; quasars : general; surveys; techniques : spectroscopic; X-rays : galaxies : clusters ID X-RAY SOURCES; ACTIVE GALACTIC NUCLEI; MEDIUM-SENSITIVITY SURVEY; GALAXY NUMBER COUNTS; HIGH-REDSHIFT; LUMINOSITY FUNCTION; NORTH SURVEY; SPECTROPHOTOMETRIC STANDARDS; COSMOLOGICAL CONSTANT; SPECTRAL PROPERTIES AB We present the results of our spectroscopic follow-up program of the X-ray sources detected in the 942 ks exposure of the Chandra Deep Field - South (CDFS). A total of 288 possible counterparts were observed at the VLT with the FORS1/FORS2 spectrographs for 251 of the 349 Chandra sources ( including three additional faint X-ray sources). Spectra and R-band images are shown for all the observed sources and R - K colors are given for most of them. Spectroscopic redshifts were obtained for 168 X-ray sources, of which 137 have both reliable optical identification and redshift estimate ( including 16 external identifications). The R < 24 observed sample comprises 161 X-ray objects (181 optical counterparts), and 126 of them have unambiguous spectroscopic identification. There are two spikes in the redshift distribution, predominantly populated by type 2 active galactic nuclei ( AGNs) but also type 1 AGN and X-ray normal galaxies: the one at z = 0.734 is fairly narrow (in redshift space) and comprises two clusters/ groups of galaxies centered on extended X-ray sources, the second one at z = 0: 674 is broader and should trace a sheetlike structure. The type 1 and type 2 populations are clearly separated in X-ray/optical diagnostics involving parameters sensitive to absorption / reddening: X-ray hardness ratio (HR), optical/near-IR color, soft X-ray flux, and optical brightness. Nevertheless, these two populations cover similar ranges of hard X-ray luminosity and absolute K magnitude, thus trace similar levels of gravitational accretion. Consequently, we introduce a new classification based solely on X-ray properties, HR, and X-ray luminosity, consistent with the unified AGN model. This X-ray classification uncovers a large fraction of optically obscured, X-ray - luminous AGNs missed by the classical optical classification. We find a similar number of X-ray type 1 and type 2 QSOs [L-X(0.5 10 keV) > 10(44) ergs s(-1)] at z > 2 (13 sources with unambiguous spectroscopic identification); most X-ray type 1 QSOs are bright, Rless than or similar to24, whereas most X-ray type 2 QSOs have Rgreater than or similar to24, which may explain the difference with the CDFN results as few spectroscopic redshifts were obtained for R> 24 CDFN X-ray counterparts. There are X-ray type 1 QSOs down to z similar to 0.5, but a strong decrease at z< 2 in the fraction of luminous X-ray type 2 QSOs may indicate a cosmic evolution of the X-ray luminosity function of the type 2 population. An X- ray spectral analysis is required to confirm this possible evolution. The red color of most X- ray type 2 AGNs could be due to dust associated with the X- ray absorbing material and/ or a substantial contribution of the host galaxy light. The latter can also be important for some redder X- ray type 1 AGNs. There is a large population of EROs ( R - K > 5) as X- ray counterparts, and their fraction strongly increases with decreasing optical flux, up to 25% for the R greater than or equal to 24 sample. They cover the whole range of X- ray hardness ratios, comprise objects of various classes ( in particular a high fraction of zgreater than or similar to1 X- ray absorbed AGNs, but also elliptical and starburst galaxies) and more than half of them should be fairly bright X- ray sources [ LX( 0: 5 10 keV) > 1042 ergs s(-1)]. Photometric redshifts will be necessary to derive the properties and evolution of the X- ray selected EROs. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Astrophysikalisches Inst Potsdam, D-14482 Potsdam, Germany. Inst Astrophys Paris, F-75014 Paris, France. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. Osserv Astron Trieste, I-34131 Trieste, Italy. Associated Univ Inc, Washington, DC 20036 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Szokoly, GP (reprint author), Max Planck Inst Extraterr Phys, Giessenbach str, D-85748 Garching, Germany. OI Nonino, Mario/0000-0001-6342-9662 NR 81 TC 410 Z9 410 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2004 VL 155 IS 2 BP 271 EP 349 DI 10.1086/424707 PG 79 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 874YH UT WOS:000225386100004 ER PT J AU Ferrier, S Powell, GVN Richardson, KS Manion, G Overton, JM Allnutt, TF Cameron, SE Mantle, K Burgess, ND Faith, DP Lamoreux, JF Kier, G Hijmans, RJ Funk, VA Cassis, GA Fisher, BL Flemons, P Lees, D Lovett, JC Van Rompaey, RSAR AF Ferrier, S Powell, GVN Richardson, KS Manion, G Overton, JM Allnutt, TF Cameron, SE Mantle, K Burgess, ND Faith, DP Lamoreux, JF Kier, G Hijmans, RJ Funk, VA Cassis, GA Fisher, BL Flemons, P Lees, D Lovett, JC Van Rompaey, RSAR TI Mapping more of terrestrial biodiversity for global conservation assessment SO BIOSCIENCE LA English DT Article DE biodiversity; global; mapping; protected areas; representativeness ID PROTECTED-AREA NETWORK; SPECIES-DIVERSITY; REGIONAL CONSERVATION; EXTINCTION RATES; HABITAT LOSS; PRIORITY; FORESTS; INFORMATICS; ECOREGIONS; PATTERNS AB Global conservation assessments require information on the distribution of biodiversity across the planet. Yet this information is often mapped at a very coarse spatial resolution relative to the scale of most land-use and management decisions. Furthermore, such mapping tends to focus selectively on better-known elements of biodiversity (e.g., vertebrates). We introduce a new approach to describing and mapping the global distribution of terrestrial biodiversity that may help to alleviate these problems. This approach focuses on estimating spatial pattern in emergent properties of biodiversity (richness and compositional turnover) rather than distributions of individual species, making it well suited to lesscr-known, yet highly diverse, biological groups. We have developed a global biodiversity model linking these properties to mapped ecoregions and fine-scale environmental surfaces. The model is being calibrated progressively using extensive biological data sets for a wide variety of taxa. We also describe an analytical approach to applying our model in global conservation assessments, illustrated with a preliminary analysis of the representativeness of the world's protected-area system. Our approach is intended to complement, not compete with, assessments based on individual species of particular conservation concern. C1 New S Wales Dept Environm & Conserv, Spatial Informat & Anal Sect, Armidale, NSW 2350, Australia. World Wildlife Fund, Conservat Sci Program, Washington, DC 20037 USA. Landcare Res, Hamilton 2001, New Zealand. Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Australian Museum, Sydney, NSW 2010, Australia. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. Univ Bonn, Nees Inst Biodivers Plants, D-53115 Bonn, Germany. Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, US Natl Herbarium, Washington, DC 20560 USA. Australian Museum, Ctr Biodivers & Conservat Res, Sydney, NSW 2000, Australia. Calif Acad Sci, San Francisco, CA 94103 USA. Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. Free Univ Brussels, Lab Plant Systemat & Phytosociol, B-1050 Brussels, Belgium. RP Ferrier, S (reprint author), New S Wales Dept Environm & Conserv, Spatial Informat & Anal Sect, Armidale, NSW 2350, Australia. EM simon.ferrier@environment.nsw.gov.au RI Cameron Devitt, Susan/E-2659-2013; Ferrier, Simon/C-1490-2009; Hijmans, Robert/N-3299-2016; OI Ferrier, Simon/0000-0001-7884-2388; Hijmans, Robert/0000-0001-5872-2872 NR 35 TC 90 Z9 95 U1 4 U2 40 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 2004 VL 54 IS 12 BP 1101 EP 1109 DI 10.1641/0006-3568(2004)054[1101:MMOTBF]2.0.CO;2 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 882KN UT WOS:000225937900008 ER PT J AU Bawa, KS Kress, WJ Nadkarni, NM Lele, S AF Bawa, KS Kress, WJ Nadkarni, NM Lele, S TI Beyond paradise - Meeting the challenges in tropical biology in the 21st century SO BIOTROPICA LA English DT Article DE biodiversity; biological research; conservation; social science; sustainable development; tropical ecosystems; tropical forests ID BIODIVERSITY; FOREST; DIVERSITY AB Tropical ecosystems support a diversity of species and ecological processes that are unparalleled anywhere else on Earth. Despite their tremendous social and scientific importance, tropical ecosystems are rapidly disappearing. To help tropical ecosystems and the human communities dependent upon them better face the challenges of the 21st century, tropical biologists must provide critical knowledge in three areas: (1) the structure and functioning of tropical ecosystems; (2) the nature and magnitude of anthropogenic effects on tropical ecosystems; and (3) the socio-economic drivers of these anthropogenic effects. To develop effective strategies for conservation, restoration, and sustainable management of tropical ecosystems, scientific perspectives must be integrated with social necessities. Three principles for guiding tropical biological research are suggested: (1) broadening the set of concerns; (2) integration of biological knowledge with the social sciences and traditional knowledge; and (3) linking science to policy and action. Four broad recommendations are proposed for immediate action in tropical biology and conservation that are fundamental to all biological and social disciplines in the tropics: (1) assemble and disseminate information on life's diversity in the tropics; (2) enhance tropical field stations and build a worldwide network to link them with tropical field biologists at their field sites; (3) bring the field of tropical biology to the tropics by strengthening institutions in tropical countries through novel partnerships between tropical and temperate zone institutions and scientists; and (4) create concrete mechanisms to increase interactions between tropical biologists, social scientists, and policy makers. C1 Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. Ashoka Trust Res Ecol & Environm, Bangalore, Karnataka, India. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Yunnan, Peoples R China. RP Bawa, KS (reprint author), Univ Massachusetts, Dept Biol, 100 Morrissey Blvd, Boston, MA 02125 USA. EM kamal.bawa@umb.edu NR 24 TC 37 Z9 41 U1 5 U2 19 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 2004 VL 36 IS 4 BP 437 EP 446 DI 10.1111/j.1744-7429.2004.tb00341.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 880TE UT WOS:000225811400001 ER PT J AU Leigh, EG Davidar, P Dick, CW Puyravaud, JP Terborgh, J ter Steege, H Wright, SJ AF Leigh, EG Davidar, P Dick, CW Puyravaud, JP Terborgh, J ter Steege, H Wright, SJ TI Why do some tropical forests have so many species of trees? SO BIOTROPICA LA English DT Review DE alpha-diversity; beta-diversity; Janzen-Connell; neutral theory; pest pressure; regional diversity; stability-time speciation ID NEOTROPICAL RAIN-FOREST; DECIDUOUS FOREST; SEED DISPERSAL; DRY FOREST; DENSITY-DEPENDENCE; GLOBAL PATTERNS; INTERSPECIFIC VARIATION; LATITUDINAL GRADIENTS; FLORISTIC COMPOSITION; PROMOTES COEXISTENCE AB Understanding why there are so many kinds of tropical trees requires learning, not only how tree species coexist, but what factors drive tree speciation and what governs a tree clade's diversification rate. Many report that hybrid sterility evolves very slowly between separated tree populations. If so, tree species rarely originate by splitting of large populations. Instead, they begin with few trees. The few studies available suggest that reproductive isolation between plant populations usually results from selection driven by lowered fitness of hybrids: speciation is usually a response to a "niche opportunity." Using Hubbell's neutral theory of forest dynamics as a null hypothesis, we show that if new tree species begin as small populations, species that are now common must have spread more quickly than chance allows. Therefore, most tree species have some setting in which they can increase when rare. Trees face trade-offs in suitability for different microhabitats, different-sized clearings, different soils and climates, and resistance to different pests. These trade-offs underlie the mechanisms maintaining alpha-diversity and species turnover. Disturbance and microhabitat specialization appear insufficient to maintain alpha-diversiry of tropical trees, although they may maintain tree diversity north of Mexico or in northern Europe. Many studies show that where trees grow readily, tree diversity is higher and temperature and rainfall are less seasonal. The few data available suggest that pest pressure is higher, maintaining higher tree diversity, where winter is absent. Tree a-diversiry is also higher in regions with more tree species, which tend to be larger, free for a longer time from major shifts of climate, or in the tropics, where there are more opportunities for local coexistence. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Pondicherry Univ, Salim Ali Sch Ecol & Environm Sci, Pondicherry 605014, India. SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. Univ Utrecht, Natl Herbarium Netherlands, NL-3584 CS Utrecht, Netherlands. RP Smithsonian Trop Res Inst, Unit 0948, APO, Miami, FL 34002 USA. RI Dick, Christopher/A-8744-2008; ter Steege, Amaz/B-5866-2011; Wright, Stuart/M-3311-2013; OI ter Steege, Amaz/0000-0002-8738-2659; Wright, Stuart/0000-0003-4260-5676; Davidar, Priya/0000-0003-2463-6743 NR 242 TC 126 Z9 135 U1 14 U2 119 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD DEC PY 2004 VL 36 IS 4 BP 447 EP 473 DI 10.1111/j.1744-7429.2004.tb00342.x PG 27 WC Ecology SC Environmental Sciences & Ecology GA 880TE UT WOS:000225811400002 ER PT J AU Meyer, CFJ Zotz, G AF Meyer, CFJ Zotz, G TI Do growth and survival of aerial roots limit the vertical distribution of hemiepiphytic aroids? SO BIOTROPICA LA English DT Article DE aerial roots; Anthurium clavigerum; Araceae; Barro Colorado Island; growth rates; hemiepiphytes; lowland tropical moist forest; Panama; Philodendron radiatum; survival analysis; vertical distribution ID WOODY HEMIEPIPHYTES; WATER RELATIONS; CLOUD FOREST; FICUS; TREE; ECOLOGY; PHOTOSYNTHESIS; EPIPHYTES; HABITAT; ARACEAE AB We tested the hypothesis that growth and survival of aerial roots impose a limit on the height at which a primary hemiepiphyte can become successfully established within tree crowns and evaluate the implications for the vertical distribution of hemiepiphytes in the forest canopy. Density and spatial distribution, and growth and survival of aerial roots were studied in two common species of hemiepiphytic Araceae, Philodendron radiatum and Anthurium clavigerum, in a lowland tropical moist forest in Panama between March and October 2001. Additionally, root growth and survival were studied both in normal, unmanipulated, and experimentally cut roots to investigate the effect of damage on root resprouting and survival. Survival analysis revealed much greater survival of aerial roots of A. clavigerum than P radiatum. In contrast, growth rates in the latter were on average about three times higher when compared to A. clavigerum. In both species, experimental cutting of the root invariably led initially to the development of dieback symptoms; however, plants responded to root damage by producing resprouts. A risk model for the two species suggests that only the fastest-growing roots of P radiatum are likely to survive long enough to reach the soil from a host branch 6.8 m high, which equals the mean height of occurrence observed for the epiphytic stage of this species at our study site. In contrast, slow-growing appressed aerial roots of A. clavigerum may never be able to establish a connection with the soil from similar heights in the canopy before roots die. Consistent with our hypothesis, A. clavigerum is found much lower in the forest (it rarely exceeds ca 5 m). C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 NR 40 TC 6 Z9 6 U1 2 U2 9 PU ASSOC TROPICAL BIOLOGY INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD DEC PY 2004 VL 36 IS 4 BP 483 EP 491 DI 10.1111/j.1744-7429.2004.tb00344.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 880TE UT WOS:000225811400004 ER PT J AU Gingerich, O AF Gingerich, O TI The Calvinist Copernicans: The reception of the new astronomy in the Dutch Republic, 1575-1750 SO BRITISH JOURNAL FOR THE HISTORY OF SCIENCE 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 CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0007-0874 J9 BRIT J HIST SCI JI Br. J. Hist. Sci. PD DEC PY 2004 VL 37 IS 135 BP 471 EP 472 DI 10.1017/S0007087404266171 PN 4 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 892RD UT WOS:000226666800011 ER PT J AU An, T Hong, XY Feng, WX Zhao, JH AF An, T Hong, XY Feng, WX Zhao, JH TI A peculiar broad line radio galaxy 1938-155: VLA observation at 90 cm SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE galaxy : quasar : individual; radio continuum : VLA ID ACTIVE GALACTIC NUCLEI; COMPLETE SAMPLE; GALAXIES; Z-LESS-THAN-0.3; SPECTROSCOPY; CORES AB We observed 1938-155, a broad line radio galaxy (BLRG), with the Very Large Array (VLA) at 90 cm with an angular resolution of 6.8" x 4.0". The source consists of two components separated by 4 arcsec (similar to 20 kpc, for H-0 = 65 km s(-1) Mpc(-l), q(0) = 0.5) along the SE-NW direction. Both components show steep-spectra with a similar spectral index alpha similar to 0.83 +/- 0.07 (S-v proportional to v(-alpha)). The bright double components are surrounded by a low-brightness cocoon. The radio properties of the two bright components are consistent with the hot spots produced by twin jets. An upper limit of similar to 0.0008 for the core dominance parameter (R) is inferred, suggesting there is no prominent radio core in the source. Assuming a modest viewing angle 30degrees, a jet velocity is estimated similar to 0.07 c, based on the jet to counter-jet brightness ratio (J). The lower limit in jet speed inferred is consistent with no Doppler beaming effect on the jet. The radio galaxy 1938-155 could be an exceptional BLRG with no prominent radio core or jet. C1 Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP An, T (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. EM antao@center.shao.ac.cn NR 14 TC 0 Z9 0 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. PD DEC PY 2004 VL 4 IS 6 BP 527 EP 532 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 895LF UT WOS:000226863000003 ER PT J AU Duckett, CN AF Duckett, CN TI Longasphaera Bechyne (Coleoptera : Chrysomelidae : Galerucinae : Alticini : Oedionychina) a new synonym of Omophoita Chevrolat SO COLEOPTERISTS BULLETIN LA English DT Article AB Examination of the holotype and comparison to other material reveal that the monotypic genus Longasphaera Bechyne is a junior synonym of Omophoita Chevrolat new synonymy. Therefore, the type species of Longasphaera, L. hispicornis Bechyne is given a new combination, O. hispicornis (Bechyne). Omophoita hispicornis is illustrated for the first time and characteristics of its labral setation that partially define the Bechyne concept of genus Omophoita are discussed. C1 Smithsonian Inst, Dept Entomol, NHB, Washington, DC 20013 USA. RP Duckett, CN (reprint author), Smithsonian Inst, Dept Entomol, NHB, MRC 187,POB 27012, Washington, DC 20013 USA. EM duckett.catherine@nmnh.si.edu NR 7 TC 0 Z9 0 U1 1 U2 3 PU COLEOPTERISTS SOC PI NATCHEZ PA PO BOX 767, NATCHEZ, MS 39121 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD DEC PY 2004 VL 58 IS 4 BP 652 EP 655 DI 10.1649/714 PG 4 WC Entomology SC Entomology GA 894CZ UT WOS:000226769200023 ER PT J AU D'Croz, L Mate, JL AF D'Croz, L Mate, JL TI Experimental responses to elevated water temperature in genotypes of the reef coral Pocillopora damicornis from upwelling and non-upwelling environments in Panama SO CORAL REEFS LA English DT Article DE thermal tolerance; coral genotypes; upwelling; ENSO sea warming ID BLEACHING PATTERNS; HEAT-SHOCK; SEA; ZOOXANTHELLAE; ECOLOGY; EVENT; HYPOTHESIS; MORTALITY; RADIATION; RECOVERY AB The authors investigated the response to experimentally elevated water temperature in genotypes of Pocillopora damicornis from three coral reefs in the upwelling Gulf of Panama and four coral reefs in the non-upwelling Gulf of Chiriqui, Panamanian Pacific. Sea-surface temperature in the Gulf of Panama declines below 20 degreesC during seasonal upwelling, while in the thermally stable Gulf of Chiriqui, the temperature ranges from 27 to 29 degreesC. Genotypes of P. damicornis from the seven locations were determined by allozyme electrophoresis. The most abundant genotype at each location was selected for a thermal tolerance experiment where corals were exposed to water temperature of 30 degreesC (1 degreesC above ambient) for 43 days. Four site coral genotypes can be uniquely differentiated by the GPI locus, two by the LGG-2 locus, and two by a combination of the MDH-1, LGG-2, and LTY-3 loci. A visual assessment of the coral condition after exposure to an elevated temperature showed that corals from localities in the non-upwelling environment retained a normal to slightly pale appearance, while corals from the upwelling environment bleached and their polyps were mostly retracted. A two-way ANOVA confirmed that corals were significantly affected by water temperature and locality. The zooxanthellae were also significantly affected by the interaction of elevated temperature and locality of the corals. Mean zooxanthellae density decreased by 25 and 55%, respectively, in experimentally heated corals from the non-upwelling and upwelling environments. Low concentrations of photosynthetic pigments per live area of the corals were the norm in corals under elevated temperature. The mean concentration of chlorophyll a per live area of the corals was reduced by 17 and 49%, respectively, in heated corals from the non-upwelling and upwelling sites. Coral genotypes from the upwelling Gulf of Panama demonstrated higher vulnerability to thermal stress than coral genotypes from the non-upwelling Gulf of Chiriqui. However, the latter showed greater differences in their responses. Thus, even at small geographic scales, corals can display different levels of tolerance to thermal stress. The difference in thermal tolerance between corals from upwelling and non-upwelling environments is concomitant with greater genetic differences in experimental corals from the thermally stable Gulf of Chiriqui compared with corals from the upwelling Gulf of Panama. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Panama, Dept Biol Marina & Limnol, Panama City, Panama. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. RP D'Croz, L (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. EM dcrozl@naos.si.edu NR 50 TC 51 Z9 52 U1 2 U2 28 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2004 VL 23 IS 4 BP 473 EP 483 DI 10.1007/s00338-004-0397-7 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 884OO UT WOS:000226095100002 ER PT J AU Hooper, ER Legendre, P Condit, R AF Hooper, ER Legendre, P Condit, R TI Factors affecting community composition of forest regeneration in deforested, abandoned land in Panama SO ECOLOGY LA English DT Article DE abandoned farmland; anthropogenic grassland; natural regeneration; panama; remnant forest; Saccharum spontaneum; secondary succession; seed dispersal; tropical forest ID BARRO COLORADO ISLAND; TROPICAL MOIST FOREST; SEED DISPERSAL; RAIN-FOREST; FLORISTIC COMPOSITION; PLANT SUCCESSION; EASTERN AMAZONIA; PIONEER TREES; PUERTO-RICO; COSTA-RICA AB We tested alternative hypotheses concerning factors affecting early forest succession and community composition in deforested and abandoned areas invaded by an exotic grass, Saccharum spontaneum, in Panama. We hypothesized three barriers to natural regeneration: (1) Saccharum competition, (2) seed dispersal limitations, and (3) fire. We measured natural free and shrub regeneration in a factorial experiment combining distances from adjacent forest. mowing treatments of the Saccharum, and a prescribed burn. To determine the applicability of the general model of neotropical succession and the nucleation model Of succession to species composition of forest regeneration in these anthropogenic grasslands in Panama the effect of time since fire and distance to remnant vegetation (isolated trees, shrubs, and large monocots) was measured. Fire significantly affected species composition and decreased species richness because most species had either their resprouting ability or seed germination inhibited by fire: the few species that had regeneration enhanced by fire dominated early successional communities. Sites differed in time since fire, ranging from 1 to 4 yr; the interaction of site and distance from the forest significantly affected community composition and the prevalence of species with different dispersal mechanisms and shade tolerance. At recently burned sites. light-dependent wind-dispersed species predominated; most were found near the forest edge. As time since fire increased, significantly more shade-tolerant, larger-animal-dispersed species were recorded, and the proximity to and species identity of remnant vegetation became more important in affecting species composition of the natural regeneration; no significant effect of distance from the forest was found at sites that were unburned for three or more years. Our results support both successional models; the temporal sequence of species composition corresponded to later stages of the general model, while the spatial distribution of species followed the nucleation model. Our results highlight the importance of effective seed dispersal in structuring successional species composition and distribution and in regaining, lost diversity resulting from frequent fires ill the Saccharum. C1 McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. Univ Montreal, Dept Sci Biol, Montreal, PQ H3C 3J7, Canada. Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Miami, FL 34002 USA. RP Hooper, ER (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM ehoop1@uic.edu NR 68 TC 56 Z9 69 U1 6 U2 47 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 DEC PY 2004 VL 85 IS 12 BP 3313 EP 3326 DI 10.1890/03-0655 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 887HV UT WOS:000226297500013 ER PT J AU Schliserman, P Ovruski, S Colin, C Norrbom, AL Aluja, M AF Schliserman, P Ovruski, S Colin, C Norrbom, AL Aluja, M TI First report of Juglans australis (Juglandaceae) as a natural host plant for Anastrepha schultzi (Diptera : Tephritidae) with notes on probable parasitism by Doryctobracon areolatus, D-Brasiliensis, Opius bellus (Braconidae) and Aganaspis pelleranoi (Figitidae) SO FLORIDA ENTOMOLOGIST LA English DT Article ID CERATITIS-CAPITATA DIPTERA; NORTHWESTERN ARGENTINA; FRATERCULUS C1 Consejo Nacl Invest Cient & Tecn, INSUE, Fdn Miguel Lillo, CIRPON, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. USDA, ARS, Systemat Entomol Lab, Smithsonian Inst, Washington, DC 20560 USA. Inst Ecol, Xalapa 91000, Veracruz, Mexico. RP Schliserman, P (reprint author), Consejo Nacl Invest Cient & Tecn, INSUE, Fdn Miguel Lillo, CIRPON, Miguel Lillo 251, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. NR 11 TC 9 Z9 9 U1 1 U2 2 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD DEC PY 2004 VL 87 IS 4 BP 597 EP 599 DI 10.1653/0015-4040(2004)087[0597:FROJAJ]2.0.CO;2 PG 3 WC Entomology SC Entomology GA 886WC UT WOS:000226262600030 ER PT J AU Kirby, MX Jackson, JBC AF Kirby, MX Jackson, JBC TI Extinction of a fast-growing oyster and changing ocean circulation in Pliocene tropical America SO GEOLOGY LA English DT Article DE Central American seaway; paleoproductivity; growth rate; oyster; Crassostrea ID STABLE-ISOTOPE SCLEROCHRONOLOGY; QUATERNARY CRASSOSTREA OYSTERS; PANAMA LAND-BRIDGE; EQUATORIAL PACIFIC; CARIBBEAN NEOGENE; BIVALVIA; ISTHMUS; MOLLUSKS; ATLANTIC; GROWTH AB Ocean circulation changed profoundly in the late Cenozoic around tropical America as a result of constriction and final closure of the Central American seaway. In response, regional planktonic productivity is thought to have decreased in the Caribbean Sea. Previous studies have shown that shallow-marine communities reflect these changes by reorganizing from a suspension-feeder-dominated community to a more carbonate-rich, phototrophic-based community. Although changes in diversity, abundance, and body size of various shallow-marine invertebrates have previously been examined, no study has specifically used growth rate in suspension feeders to examine the effect that changes in ocean circulation may have had on shallow-marine communities. Here we show that a fast-growing oyster went extinct concurrently with changes in ocean circulation and planktonic productivity in the Pliocene. Faster-growing Crassostrea cahobasensis went extinct, whereas slower-growing Crassostrea virginica and columbiensis survived to the Holocene. Miocene-Pliocene C. cahobasensis grew 522 % faster in shell carbonate and 251 % faster in biomass relative to Quaternary C. virginica and C. columbiensis. Although differences in growth are due to proximate differences in environment, the disappearance of faster-growing C. cahobasensis from shallow-marine environments and the continued survival of slower-growing C. virginica and C. columbiensis in marginal-marine environments (e.g., estuaries, lagoons) is consistent with the view that concurrent changes in ocean circulation and declining primary production resulted in the restriction of Crassostrea to marginal-marine environments. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. RP Kirby, MX (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 2072, Balboa, Panama. NR 47 TC 18 Z9 19 U1 0 U2 11 PU GEOLOGICAL SOC AMERICA, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD DEC PY 2004 VL 32 IS 12 BP 1025 EP 1028 DI 10.1130/G21039.1 PG 4 WC Geology SC Geology GA 877QN UT WOS:000225585200005 ER PT J AU Niemi, NA Wernicke, BP Friedrich, AM Simons, M Bennett, RA Davis, JL AF Niemi, NA Wernicke, BP Friedrich, AM Simons, M Bennett, RA Davis, JL TI BARGEN continuous GPS data across the eastern Basin and Range province, and implications for fault system dynamics SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Review DE continental deformation; fault slip; normal faulting; Quaternary; satellite geodesy; stress distribution ID WESTERN UNITED-STATES; SEISMIC-REFLECTION DATA; NORTHERN SNAKE RANGE; SAN-ANDREAS FAULT; GLOBAL POSITIONING SYSTEM; SEVIER DESERT REFLECTION; ANGLE NORMAL FAULTS; WASATCH FAULT; CENTRAL UTAH; GREAT-BASIN AB We collected data from a transect of continuous Global Positioning System (GPS) sites across the eastern Basin and Range province at latitude 39degreesN from 1997-2000. Intersite velocities define a region similar to350 km wide of broadly distributed strain accumulation at similar to10 nstr yr(-1). On the western margin of the region, site EGAN, similar to10 km north of Ely, Nevada, moved at a rate of 3.9 +/- 0.2 mm yr(-1) to the west relative to site CAST, which is on the Colorado Plateau. Velocities of most sites to the west of Ely moved at an average rate of similar to3 mm yr(-1) relative to CAST, defining an area across central Nevada that does not appear to be extending significantly. The late Quaternary geological velocity field, derived using seismic reflection and neotectonic data, indicates a maximum velocity of EGAN with respect to the Colorado Plateau of similar to4 mm yr(-1), also distributed relatively evenly across the region. The geodetic and late Quaternary geological velocity fields, therefore, are consistent, but strain release on the Sevier Desert detachment and the Wasatch fault appears to have been anomalously high in the Holocene. Previous models suggesting horizontal displacement rates in the eastern Basin and Range near 3 mm yr(-1), which focused mainly along the Wasatch zone and Intermountain seismic belt, may overestimate the Holocene Wasatch rate by at least 50 per cent and the Quaternary rate by nearly an order of magnitude, while ignoring potentially major seismogenic faults further to the west. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Niemi, NA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM niemi@gps.caltech.edu RI Niemi, Nathan/A-9996-2011; Friedrich, Anke/G-2921-2011; Davis, James/D-8766-2013; OI Friedrich, Anke/0000-0002-6938-8563; Davis, James/0000-0003-3057-477X; Niemi, Nathan/0000-0002-3380-3024; Simons, Mark/0000-0003-1412-6395 NR 127 TC 43 Z9 44 U1 0 U2 15 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD DEC PY 2004 VL 159 IS 3 BP 842 EP 862 DI 10.1111/j.1365-246X.2004.02454.x PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 873FA UT WOS:000225264100002 ER PT J AU Savage, JM Hollingsworth, BD Lips, KR Jaslosw, AP AF Savage, JM Hollingsworth, BD Lips, KR Jaslosw, AP TI A new species of rainfrog (genus Eleutherodactylus) from the Serrania de Tabasara, west-central Panama and reanalysis of the fitzingeri species group SO HERPETOLOGICA LA English DT Article DE Anura; Eleutherodactylus fitzingeri species group; Leptodactylidae; new species; Panama ID PHYLOGENETIC-RELATIONSHIPS; RETENTION INDEX; ALLOZYME DATA; GROUP ANURA; LEPTODACTYLIDAE; AMPHIBIA; FROGS; SYSTEMATICS; CONFIDENCE; RUGULOSUS AB We describe a new species of rainfrog of the Eleutherodactylus fitzingeri species group from central Panama. This species is most similar to members of the E. melanostictus subgroup and can be distinguished from other members of the E. fitzingeri group from Lower Central America by a combination of characters, including a large supraocular tubercle, barred thigh pattern, a granulate venter, marked sexual dimorphism in the tympanic membrane, and basal toe webbing. We analyzed a data matrix of 24 allozyme, morphological, and karyological characters, following the phylogenetic analysis of Miyamoto (1986), and included four additional characters. The 12 species of the E. fitzingeri group are included, in addition to the new species. The relative phylogenetic position of two species, E. emcelae and E. phasma, are proposed for the first time. The new species is hypothesized to be a member of the E. melanostictus subgroup, which contains the predominantly montane species E. melanostictus, E. rayo, E. emcelae, E. monnichorum, and E. cuaquero. C1 So Illinois Univ, Dept Zool, Carbondale, IL 62901 USA. San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. San Diego Nat Hist Museum, Dept Herpetol, San Diego, CA 92112 USA. Rhodes Coll, Dept Biol, Memphis, TN 38112 USA. Smithsonian Trop Res Inst, Carbondale, IL 62901 USA. RP Lips, KR (reprint author), So Illinois Univ, Dept Zool, Carbondale, IL 62901 USA. EM klips@zoology.siu.edu OI Lips, Karen/0000-0002-2719-1551 NR 35 TC 11 Z9 12 U1 0 U2 0 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0018-0831 EI 1938-5099 J9 HERPETOLOGICA JI Herpetologica PD DEC PY 2004 VL 60 IS 4 BP 519 EP 529 DI 10.1655/03-29 PG 11 WC Zoology SC Zoology GA 879CQ UT WOS:000225694400014 ER PT J AU Collin, R AF Collin, R TI Effects of conspecific associations on size at sex change in calyptraeid gastropods SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Trop Res Inst, Balboa, Panama. EM collinr@naos.si.edu RI Collin, Rachel/G-2001-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 538 EP 538 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400114 ER PT J AU Curtin, AJ Zug, GR Avery, HW Spotila, JR AF Curtin, AJ Zug, GR Avery, HW Spotila, JR TI Bone growth patterns as indicators of life history parameters in desert tortoise (Gopherus agassizii) populations SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Inst, Washington, DC 20560 USA. Drexel Univ, Philadelphia, PA 19104 USA. Natl Museum Nat Hist, Washington, DC 20560 USA. EM ajcurtin@drexel.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 542 EP 542 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400130 ER PT J AU Head, JJ AF Head, JJ TI Ecological and phylogenetic variation in segmentation in snakes SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Inst, Washington, DC 20560 USA. EM head.jason@nmnh.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 566 EP 566 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400225 ER PT J AU Kim, TW Rissanen, R Rebeiro, P Christy, JH Choe, JC AF Kim, TW Rissanen, R Rebeiro, P Christy, JH Choe, JC TI Sexual differences in the affects of supplimental food on the semilunar reproductive rhythms of an intertidal crab SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Seoul Natl Univ, Seoul 151, South Korea. Univ Panama, Panama City, Panama. Univ Nacl Mar del Plata, Mar Del Plata, Argentina. Smithsonian Trop Res Inst, Balboa, Panama. EM ocean74@snu.ac.kr NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 583 EP 583 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400291 ER PT J AU Lombardo, R Christy, JH Rissanen, R AF Lombardo, R Christy, JH Rissanen, R TI Social monogamy in a simultaneous hermaphrodite SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Trop Res Inst, Balboa, Panama. EM christyj@si.edu NR 0 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 594 EP 594 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400335 ER PT J AU Maslakova, S Martindale, M Norenburg, J AF Maslakova, S Martindale, M Norenburg, J TI Hidden trochophore in nemertean development revealed by confocal microscopy and cell lineage analysis SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 George Washington Univ, Washington, DC 20052 USA. Univ Hawaii, Honolulu, HI 96822 USA. Smithsonian Inst, Washington, DC 20560 USA. NMNH, Washington, DC USA. EM maslak@gwu.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 598 EP 598 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721400354 ER PT J AU Santagata, S AF Santagata, S TI Evolutionary trends in the larval anatomy of the bryozoa SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. EM santagata@sms.si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 635 EP 635 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721401041 ER PT J AU Zanol, J Fauchald, K AF Zanol, J Fauchald, K TI Looking for more morphological information, a study of morphological characters in Eunicidae (Eunicida, Polychaeta, Annelida) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 George Washington Univ, Washington, DC 20052 USA. Smithsonian Inst, Washington, DC 20560 USA. EM jzanol@gwu.edu NR 0 TC 0 Z9 0 U1 1 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 670 EP 670 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721401184 ER PT J AU Croll, RP Hochberg, R AF Croll, RP Hochberg, R TI Neomeniomorpha-solenogastres (Aplacophora): Insights into the neuromuscular system of primitive mollusca SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Dalhousie Univ, Halifax, NS B3H 3J5, Canada. Smithsonian Marine Stn, Ft Pierce, FL USA. EM Hochberg_Rick@yahoo.com RI Croll, Roger/E-2011-2011 NR 0 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 685 EP 685 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721401242 ER PT J AU Hochberg, R AF Hochberg, R TI Functional morphology of jumping appendages in planktonic rotifera: Ultrastructure and neuromuscular control of spines in Filinia longisetae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. EM Hochberg_Rick@yahoo.com NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 706 EP 706 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721401324 ER PT J AU Rice, ME Schulze, A AF Rice, ME Schulze, A TI Molecular and morphological species identification of pelagic sipunculan larvae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 04-08, 2005 CL San Diego, CA SP Soc Integrat & Comparat Biol C1 Smithsonian Marine Stn, Ft Pierce, FL USA. EM schulze@sms.si.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2004 VL 44 IS 6 BP 740 EP 740 PG 1 WC Zoology SC Zoology GA 893LU UT WOS:000226721401462 ER PT J AU Scelzo, MA Mantelatto, FL Tudge, CC AF Scelzo, MA Mantelatto, FL Tudge, CC TI Spermatophore morphology of the endemic hermit crab Loxopagurus loxochelis (Anomura, Diogenidae) from the southwestern Atlantic - Brazil and Argentina SO INVERTEBRATE REPRODUCTION & DEVELOPMENT LA English DT Article DE spermatophore; hermit crab; Diogenidae; reproduction ID MATURE SPERMATOZOON; DECAPODA; PAGUROIDEA; PAGURIDAE; CRUSTACEA; ULTRASTRUCTURE; COENOBITIDAE; FAMILIES; UBATUBA; GENUS AB The spermatophore morphology of the endemic and monotypic hermit crab Loxopaguras loxochelis from the southwestern Atlantic is described. The spermatophores show similarities with those described for other members of the family Diogenidae (especially the genus Clibanarius), and are composed of three major regions: a sperm-filled, circular flat ampulla; a columnar stalk; and a pedestal. The morphology and size of the spermatophore of L. loxochelis. along with a distinguishable constriction or neck that penetrates almost half way into the base of the ampulla, are characteristic of this species. The size of the spermatophore is related to hermit crab size. Direct relationships were found between the spermatophore ampulla width, total length, and peduncle length with carapace length of the hermit crab. These morphological characteristics and size of the spermatophore of L. loxochelis are species-specific, distinguishing them from other members of the family Diogenidae, and can be used to infer phylogenetic relationships-among them. C1 Univ Nacl Mar Del Plata, CONICET, FCEyN, Dept Ciencias Marinas, RA-3350 Mar Del Plata, Argentina. Univ Sao Paulo, FFCLRP, Dept Biochem, BR-14049 Ribeirao Preto, Brazil. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. RP Scelzo, MA (reprint author), Univ Nacl Mar Del Plata, CONICET, FCEyN, Dept Ciencias Marinas, B7600AYL, RA-3350 Mar Del Plata, Argentina. EM mascelzo@mdp.edu.ar RI Mantelatto, Fernando/H-2695-2012 OI Mantelatto, Fernando/0000-0002-8497-187X NR 51 TC 23 Z9 23 U1 0 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0792-4259 EI 2157-0272 J9 INVERTEBR REPROD DEV JI Invertebr. Reprod. Dev. PD DEC PY 2004 VL 46 IS 1 BP 1 EP 9 DI 10.1080/07924259.2004.9652599 PG 9 WC Reproductive Biology; Zoology SC Reproductive Biology; Zoology GA 891YY UT WOS:000226618100001 ER PT J AU Fortunato, H AF Fortunato, H TI Reproductive strategies in gastropods across the Panama seaway SO INVERTEBRATE REPRODUCTION & DEVELOPMENT LA English DT Article; Proceedings Paper CT Symposium on Reproduction and Developmenr Patterns in Molluscs held at the World Congress of Malacology CY JUL 11-16, 2004 CL Perth, AUSTRALIA DE mollusks; Gastropoda; larval development; Panama gateway ID GALAPAGOS-ISLANDS ECUADOR; REEF CORAL REPRODUCTION; LARVAL DEVELOPMENT; MARINE-INVERTEBRATES; EASTERN PACIFIC; COSTA-RICA; PROSOBRANCH GASTROPODS; SPECIES LONGEVITY; EGG SIZE; ECOLOGY AB Biogeographic patterns of marine organisms can be related to historical or ecological factors. In either case, an organism's dispersal capabilities may have an impact on rates of speciation, extinction, and species longevity. One way to assess these factors is to compare patterns and trends in developmental modes among closely related taxa across different environments. The Caribbean and the eastern Pacific differ greatly in primary productivity and seasonality. The latter is more seasonal and productive, and these differences have existed for several million years. Likewise, reproductive propagules (eggs, larvae) of echinoderms, corals, and bryozoans are smaller or mostly planktonic in the eastern Pacific when compared with the Caribbean. T his is probably due to the greater seasonality and higher productivity of the eastern Pacific, as opposed to the more stable, less productive Caribbean. This study used protoconch morphology to infer developmental patterns for 84 recent species of columbellid gastropods of the Strombina group, Conus, Oliva, and Olivella. Planktotrophy predominates within the eastern Pacific, whereas Caribbean species show mostly non-planktotrophic development. Thus mollusks exhibit the same differences between these two oceans as the other phyla. Most studies of evolutionary trends in modes of development have been done for north Atlantic and Mediterranean species. There, non-planktotrophic development increases with latitude and bathymetry. However, our data from the Eastern Pacific indicates that the widely reported tendency to evolve from planktotrophic to direct development may reflect changing environmental conditions in the Atlantic rather than an inevitable evolutionary trend. These results agree with a few studies for the south Atlantic and Antarctic regions that indicate that latitudinal and bathymetric constraints on developmental modes are probably much more complex than initially assumed. Moreover, the effects imposed by phylogeny on life histories can either direct or constrain the observed shifts in developmental types. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Fortunato, H (reprint author), Smithsonian Trop Res Inst, POB 169, Balboa, Panama. EM fortunae@ancon.si.edu NR 47 TC 8 Z9 8 U1 0 U2 8 PU INT SCIENCE SERVICES/BALABAN PUBLISHERS PI REHOVOT PA PO BOX 2039, REHOVOT 76120, ISRAEL SN 0792-4259 J9 INVERTEBR REPROD DEV JI Invertebr. Reprod. Dev. PD DEC PY 2004 VL 46 IS 2-3 BP 139 EP 148 DI 10.1080/07924259.2004.9652617 PG 10 WC Reproductive Biology; Zoology SC Reproductive Biology; Zoology GA 930DZ UT WOS:000229397300008 ER PT J AU Maksel, R AF Maksel, R TI The festive state: Race, ethnicity, and nationalism as cultural performance SO JOURNAL OF AMERICAN FOLKLORE LA English DT Book Review C1 Smithsonian Magazine, Washington, DC USA. RP Maksel, R (reprint author), Smithsonian Magazine, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER FOLKLORE SOC PI ARLINGTON PA 4350 NORTH FAIRFAX DR, STE 640, ARLINGTON, VA 22203 USA SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD WIN PY 2004 VL 117 IS 463 BP 105 EP 106 DI 10.1353/jaf.2004.0017 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 769TT UT WOS:000188666400011 ER PT J AU Belanus, BJ AF Belanus, BJ TI Cyberpl@y: Communicating online SO JOURNAL OF AMERICAN FOLKLORE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Belanus, BJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER FOLKLORE SOC PI ARLINGTON PA 4350 NORTH FAIRFAX DR, STE 640, ARLINGTON, VA 22203 USA SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD WIN PY 2004 VL 117 IS 463 BP 119 EP 120 DI 10.1353/jaf.2004.0005 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 769TT UT WOS:000188666400027 ER PT J AU Sanchez, C Bush, M Montali, R AF Sanchez, C Bush, M Montali, R TI Polycystic kidney disease associated with unilateral lameness in a northern pintail (Anas acuta) SO JOURNAL OF AVIAN MEDICINE AND SURGERY LA English DT Article DE polycystic disease; kidney disease; lameness; sacral nerve plexus; avian; northern pintail; Anas acuta ID CATS; ULTRASONOGRAPHY AB A captive 10-year-old female northern pintail (Alias acuta) with a history Of unilateral lameness was diagnosed at necropsy with polycystic disease most severely affecting the right kidney. The lameness was attributed to pressure on the sacral nerve plexus caused by the Unusually large cyst arising from the right kidney. Polycystic kidney disease previously has been considered an incidental finding in avian species and has only been reported in a pigeon. The clinical significance of polycystic kidney disease in this pintail was attributed to the mechanical pressure caused by the cyst rather than renal dysfunction. C1 Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. Smithsonian Conversat & Res Ctr, Dept Vet Serv, Front Royal, VA 22630 USA. RP Sanchez, C (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA. NR 13 TC 2 Z9 2 U1 0 U2 1 PU ASSOC AVIAN VETERINARIANS PI BOCA RATON PA PO BOX 811720, BOCA RATON, FL 33481 USA SN 1082-6742 J9 J AVIAN MED SURG JI J. Avian Med. Surg. PD DEC PY 2004 VL 18 IS 4 BP 257 EP 262 DI 10.1647/2003-030 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 012OF UT WOS:000235347800005 ER PT J AU Lewis, SL Phillips, OL Sheil, D Vinceti, B Baker, TR Brown, S Graham, AW Higuchi, N Hilbert, DW Laurance, WF Lejoly, J Malhi, Y Monteagudo, A Vargas, PN Sonke, B Supardi, N Terborgh, JW Martinez, RV AF Lewis, SL Phillips, OL Sheil, D Vinceti, B Baker, TR Brown, S Graham, AW Higuchi, N Hilbert, DW Laurance, WF Lejoly, J Malhi, Y Monteagudo, A Vargas, PN Sonke, B Supardi, N Terborgh, JW Martinez, RV TI Tropical forest tree mortality, recruitment and turnover rates: calculation, interpretation and comparison when census intervals vary SO JOURNAL OF ECOLOGY LA English DT Article DE carbon dioxide; global environmental change; long-term monitoring; modelling; neotropics; palaeotropics; permanent sample plot; rain forest; tree; tropical forest dynamics ID RAIN-FOREST; EVALUATING TURNOVER; DYNAMICS; DIVERSITY; AMAZON; SCALE; PLOTS; COMMUNITIES; VEGETATION; BIOMASS AB 1. Mathematical proofs show that rate estimates, for example of mortality and recruitment, will decrease with increasing census interval when obtained from censuses of non-homogeneous populations. This census interval effect could be confounding or perhaps even driving conclusions from comparative studies involving such rate estimates. 2. We quantify this artefact for tropical forest trees, develop correction methods and re-assess some previously published conclusions about forest dynamics. 3. Mortality rates of > 50 species at each of seven sites in Africa, Latin America, Asia and Australia were used as subpopulations to simulate stand-level mortality rates in a heterogeneous population when census intervals varied: all sites showed decreasing stand mortality rates with increasing census interval length. 4. Stand-level mortality rates from 14 multicensus long-term forest plots from Africa, Latin America, Asia and Australia also showed that, on average, mortality rates decreased with increasing census interval length. 5. Mortality, recruitment or turnover rates with differing census interval lengths can be compared using the mean rate of decline from the 14 long-term plots to standardize estimates to a common census length using lambda(corr) = lambda x t(0.08), where lambda is the rate and t is time between censuses in years. This simple general correction should reduce the bias associated with census interval variation, where it is unavoidable. 6. Re-analysis of published results shows that the pan-tropical increase in stem turnover rates over the late 20th century cannot be attributed to combining data with differing census intervals. In addition, after correction, Old World tropical forests do not have significantly lower turnover rates than New World sites, as previously reported. Our pan-tropical best estimate adjusted stem turnover rate is 1.81 +/- 0.16% a(-1) (mean +/- 95% CI, n = 65). 7. As differing census intervals affect comparisons of mortality, recruitment and turnover rates, and can lead to erroneous conclusions, standardized field methods, the calculation of local correction factors at sites where adequate data are available, or the use of our general standardizing formula to take account of sample intervals, are to be recommended. C1 Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JU, Midlothian, Scotland. Ctr Int Forestry Res, Jakarta 10065, Indonesia. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Winrock Int Livestock Res & Training Ctr, Arlington, VA 22209 USA. CSIRO, Trop Forest Res Ctr, Atherton, Qld, Australia. Cooperat Res Ctr Rainforest Ecol & Management, Atherton, Qld, Australia. Inst Nacl Pesquisas Amazonicas, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Inst Nacl Pesquisas Amazonicas, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Free Univ Brussels, Lab Bot Systemat Phytosociol, Brussels, Belgium. Univ Nacl San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. Jardin Bot Missouri, Proyecto Flora Peru, Oxampampa, Peru. Univ Yaounde I, Ecole Normale Super Yaounde, Yaounde, Cameroon. Forest Res Inst Malaysia, Forest Environm Div, Forest Ecol Unit, Kuala Lumpur 52109, Malaysia. Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. RP Lewis, SL (reprint author), Univ Leeds, Sch Geog, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. EM slewis@pobox.com RI Hilbert, David/A-3796-2008; Oktafian, Yuan/C-2541-2008; Laurance, William/B-2709-2012; Sheil, Douglas/H-1466-2012; Phillips, Oliver/A-1523-2011; Sheil, Douglas/A-3867-2015; OI Phillips, Oliver/0000-0002-8993-6168; Sheil, Douglas/0000-0002-1166-6591; Lewis, Simon/0000-0002-8066-6851 NR 49 TC 75 Z9 80 U1 3 U2 43 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0022-0477 J9 J ECOL JI J. Ecol. PD DEC PY 2004 VL 92 IS 6 BP 929 EP 944 DI 10.1111/j.0022-0477.2004.00923.x PG 16 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 878FG UT WOS:000225631400001 ER PT J AU Weinbeer, M Kalko, EKV AF Weinbeer, M Kalko, EKV TI Morphological characteristics predict alternate foraging strategy and microhabitat selection in the orange-bellied bat, Lampronycteris brachyotis SO JOURNAL OF MAMMALOGY LA English DT Article DE Barro Colorado island; bat community; coexistence; Lampronycteris brachyotis; Neotropics; Panama; phyllostomidae; spatial use; telemetry ID HOME-RANGE; COMMUNITY STRUCTURE; GLEANING BATS; FLIGHT; BEHAVIOR; GLOSSOPHAGINAE; PHYLLOSTOMIDAE; ECHOLOCATION; ECOLOGY; CANOPY AB Neotropical bat species may coexist because they forage in different places or in different ways. The small insectivorous orange-bellied bat, Lampronycteris brachyotis (Phyllostomidae), differs from coexisting gleaners in key ecomorphological characteristics, including longer, narrower wings and smaller ears. Using telemetry, we measured range size, range use, and activity patterns, and assessed habitat preferences for 9 individuals for 50 nights over 4 months on Barro Colorado Island, Panama. The bats spent the night in individual, medium-sized (22-27 ha) foraging areas within forested regions close to shorelines, up to 4 km away from the day roost. Each bat spent most of its time in a small (3-5 ha) core area. Foraging flights ranged from a few s to more than 70 min. Total flight time per night averaged 3.5 h and flight distance was estimated to be 60 km. There were no distinct activity peaks. Our tracking data suggest that L. brachyotis primarily forages in the canopy, where it gleans insects from vegetation in a combination of perch hunting and continuous flight. This species may also catch insects in air above the canopy. This unique behaviour among gleaning insectivorous phyllostomids corroborates our hypothesis that morphological adaptations combined with behavioural flexibility reflect distinct differences in foraging strategies and microhabitat selection. We conclude that differential use of space and hunting strategies promotes coexistence among the species-rich guild of Neotropical insectivorous gleaning bats. C1 Univ Ulm, D-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Kalko, EKV (reprint author), Univ Ulm, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM elisabeth.kalko@biologie.uni-ulm.de NR 58 TC 23 Z9 24 U1 1 U2 12 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 DEC PY 2004 VL 85 IS 6 BP 1116 EP 1123 DI 10.1644/BWG-206.1 PG 8 WC Zoology SC Zoology GA 882PM UT WOS:000225950800011 ER PT J AU Xu, LH Muller, HSP van der Tak, FFS Thorwirth, S AF Xu, LH Muller, HSP van der Tak, FFS Thorwirth, S TI The millimeter-wave spectrum of perdeuterated methanol, CD3OD SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE methanol; CD3OD; millimeter-wave spectroscopy; rotational spectroscopy; Hamiltonian; internal rotation; interstellar molecules; deuteration ID TRIPLY DEUTERATED AMMONIA; EXCITED TORSIONAL STATES; TERAHERTZ REGION; GLOBAL FIT; ROTATIONAL TRANSITIONS; 1ST DETECTION; SPECTROSCOPY; MOLECULES; CORES; H2D+ AB In order to provide accurate rest frequencies for astronomical searches, the spectrum of percleuterated methanol, CD3OD, has been measured in the frequency range 62-233 GHz. A total of 379 lines was measured from rotational states up to J = 20 and K = 10 within the ground and first excited torsional states (v, = 0 and 1). Using a one-dimensional torsion-rotation Hamiltonian, the lines were fitted to measurement accuracy (< 30 kHz). (C) 2004 Elsevier Inc. All rights reserved. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ New Brunswick, Dept Phys Sci, St John, NB E2L 4L5, Canada. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Harvard Univ, Dept Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van der Tak, FFS (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM vdtak@mpifr-bonn.mpg.de RI Thorwirth, Sven/C-6217-2011; Xu, Li-Hong/J-5095-2015; OI Thorwirth, Sven/0000-0001-8200-6710; Mueller, Holger/0000-0002-0183-8927 NR 32 TC 8 Z9 8 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD DEC PY 2004 VL 228 IS 2 BP 220 EP 229 DI 10.1016/j.jms.2004.04.015 PG 10 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 869ES UT WOS:000224966800002 ER PT J AU Suarez-Morales, E Rayner, NA AF Suarez-Morales, E Rayner, NA TI New records for the South African diaptomid fauna with a complementary description of Paradiaptomus lamellatus Sars (Copepoda, Diaptomidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE Calanoida; copepods; new records; freshwater fauna; biogeography; limnobiology; redescription; South Africa AB Information on the freshwater calanoid fauna of South Africa is incomplete. Recent collections from several environmental sites in the Western Cape Province of South Africa yielded new records of diaptomid copepods. Material was collected from more than 30 different localities. Species recorded from these sites were: Lovenula simplex Kiefer, Paradiaptomus lamellatus Sars, P. hameri Rayner, Metadiaptomus purcelli (Sars) and M. capensis (Sars). New information on the distributional and ecological ranges of these species is provided as well. Paradiaptomus lamellatus, the type species of the genus, was described more than a century ago by G. O. Sars (1895) based on material collected in South Africa by W. F. Purcell. Although in recent years other closely related Paradiaptomus species have been described using a wider set of characters, P. lamellatus has not been redescribed. The type specimens of this species are lost; hence, in the light of current taxonomic and biogeographical knowledge, it is important that the type species of Paradiaptomus (P. lamellatus ) be redescribed. This redescription was based on male and female specimens of P. lamellatus collected from Groot Rondevlei, a brown water vlei located on the Cape peninsula of South Africa. New characters are described and depicted including details of the mouth appendages, furcal rami, and male and female fifth legs. Comments on intraspecific variability and habitat preference are included. C1 Colegio Frontera Sur Chetumal, Chetumal 77000, Quintana Roo, Mexico. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Univ Durban Westville, Dept Zool, ZA-4000 Durban, South Africa. RP Suarez-Morales, E (reprint author), Colegio Frontera Sur Chetumal, AP 424, Chetumal 77000, Quintana Roo, Mexico. EM esuarez@ecosur-qroo.mx NR 14 TC 1 Z9 1 U1 1 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. PD DEC PY 2004 VL 38 IS 22 BP 2803 EP 2819 DI 10.1080/00222930310001657676 PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 827WC UT WOS:000221933400001 ER PT J AU Miller, AW Chang, AL Cosentino-Manning, N Ruiz, GM AF Miller, AW Chang, AL Cosentino-Manning, N Ruiz, GM TI A new record and eradication of the Northern Atlantic alga Ascophyllum nodosum (Phaeophyceae) from San Francisco Bay, California, USA SO JOURNAL OF PHYCOLOGY LA English DT Article DE eradication; exotic; fucoid; invasion; marine; nonindigenous species AB A new record of the Northern Atlantic fucoid Ascophyllum nodosum (L.) Le Jolis (Knotted wrack) was discovered on a shoreline in San Francisco Bay, California during a survey of intertidal habitats in 2001-2002. The alga showed no signs of deterioration 2.5 months after its initial detection. The healthy condition, presence of receptacles with developing oogonia, potential for asexual reproduction, and ability to withstand environmental conditions, both inside the Bay and on the outer Pacific coast, prompted a multiagency eradication effort. Given the relatively small area of shoreline inhabited by the alga, in combination with its absence in 125 other surveyed locations, we decided that manual removal of the seaweed would be the most environmentally sensitive yet effective eradication approach. No A. nodosum has been detected at the site since December 2002, and the species is thought to have been locally eradicated. The site continues to be monitored to assess the success of the eradication efforts. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. NOAA, Fisheries Restorat Ctr, Santa Rosa, CA 95404 USA. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM millerw@si.edu RI Chang, Andrew/J-8058-2016; OI Chang, Andrew/0000-0002-7870-285X; Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X NR 13 TC 22 Z9 23 U1 0 U2 8 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD DEC PY 2004 VL 40 IS 6 BP 1028 EP 1031 DI 10.1111/j.1529-8817.2004.04081.x PG 4 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 878GB UT WOS:000225633600003 ER PT J AU Hochberg, R AF Hochberg, R TI Smithsoniarhynches, a new genus of interstitial gnathorhynchidae (Platyhelminthes : Kalyptorhynchia) from Mosquito Lagoon and Indian River Lagoon, Florida SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article AB A new genus of marine, interstitial schizorhynch (Platyhelminthes: Kalyptorhynchia) is described from sediment collected in Mosquito Lagoon and Indian River Lagoon, Florida, USA. Smithsoniarhynches is characterized by the presence of proboscis hooks constructed of ten individual spine-like teeth that emerge separately from a basal plate. Histology and confocal laser scanning microscopy arc used to reveal additional details of the proboscis musculature and reproductive anatomy. The type species, Smithsoniarhynches sherryeedae sp. nov., is characterized by well-developed proboscis pads, four pairs of proboscis retractor muscles, and a pharynx in the midbody region. The male reproductive system consists of an anterior testis, Muscular seminal vesicle, copulatory bulb lined with spiral and circular muscles, and a sclerotic stylet. The female system consists of an unpaired vitellarium, Ovary, uterus and bursa. The bursa tissue Surrounds a muscular bursa seminalis with distinct sphincter muscles. The new genus is compared with the known 11 genera within the Gnathorhynchidae to establish a tentative hypothesis of relationships. C1 Smithsonian Marine Stn, Ft Pierce, FL 34981 USA. RP Hochberg, R (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34981 USA. EM Hochberg.Rick@yahoo.com NR 13 TC 4 Z9 4 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD DEC PY 2004 VL 84 IS 6 BP 1143 EP 1149 DI 10.1017/S0025315404010586h PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 884HK UT WOS:000226075300005 ER PT J AU Abebe, E Grizzle, RE Hope, D Thomas, WK AF Abebe, E Grizzle, RE Hope, D Thomas, WK TI Nematode diversity in the Gulf of Maine, USA, and a Web-accessible, relational database SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article ID DEEP-SEA; SPECIES-DIVERSITY; MARINE NEMATODES; COMMUNITY STRUCTURE; NORTH-SEA; ASSEMBLAGES; BIODIVERSITY; PATTERNS; MEIOFAUNA AB Nematode assemblages were studied from four sublittoral sites at 50-56 in depth in the Gulf of Maine, north-eastern coast of the USA, within the context of an open ocean aquaculture experimental site. All four sites, two potential impact and two control sites, had a similar muddy-sand bottom and low organic content. Seventy genera in 27 families were recorded from a total of 1072 individuals. All but one taxa could be related to known genera. Family Comesomatidae was the most dominant with close to a third (27.6%) of the total individuals. At the genus level Sabatieria and Setosaballeria were most dominant with a quarter of the total number of individuals. Composition of dominant families from the Gulf Of Maine differed front all hitherto reported sublittoral or deep-sea communities front both sides of the Atlantic, and most similar with European estuaries. Nematode diversity at the genus-level was reasonably high and was comparable with Mediterranean samples. Most diversity indices ordered the four sites similarly with Site 2 as the most diverse followed by Site 5 and then Site 6. By contrast the relative diversity of Site 4 depended on the index employed and its k-dominance curve crossed that of the others. Furthermore based on clustering the community at Site 4 was least similar to the others. Although these observations could be related to the fact that Site 4 is within the expected impact zone of the fish cage, the low number of fish introduced by the time of sampling and the lack of any difference in the maturity index among all the sites argue that these results can be considered before-impact data for further monitoring of the open ocean aquaculture experiment. A new paradigm where morphological information is documented and communicated using digital multifocal images is introduced. Each video image is comparable with visualization of a specimen under a microscope where the movie can be played back and forth to mimic focusing through a specimen. Web-based and openly accessible digital multifocal images were used to document and effectively communicate the morphology of all the identified genera in this study. This approach for documenting and communicating survey results is proposed as a benchmark for future similar studies that would enhance standardization and quality control of meiofaunal taxonomy, ecology and biodiversity studies. C1 Univ New Hampshire, Hubbard Ctr Genome Studies, Durham, NH 03824 USA. Univ New Hampshire, Dept Zool, Durham, NH 03824 USA. Univ New Hampshire, Dept Zool, Jackson Estuarine Lab, Durham, NH 03824 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. RP Abebe, E (reprint author), Univ New Hampshire, Hubbard Ctr Genome Studies, 35 Colovos Rd,Gregg Hall 4th Floor, Durham, NH 03824 USA. EM Eyualem@unh.edu NR 35 TC 4 Z9 4 U1 1 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD DEC PY 2004 VL 84 IS 6 BP 1159 EP 1167 DI 10.1017/S0025315404010604h PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 884HK UT WOS:000226075300007 ER PT J AU Linder, A Cairns, SD Guzman, HM AF Linder, A Cairns, SD Guzman, HM TI Distichopora robusta sp. nov., the first shallow-water stylasterid (Cnidaria : Hydrozoa : Stylasteridae) form the tropical eastern Pacific (vol 84, 944, 2004) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Correction C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Cairns, SD (reprint author), Smithsonian Inst, NMNH, Dept Zool, PO Box 37012,W-329,MRC-0163, Washington, DC 20013 USA. EM alberto.linder@duke.edu; Cairns.Stephen@NMNH.SI.EDU; guzmanh@naos.si.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD DEC PY 2004 VL 84 IS 6 BP 1254 EP 1255 PG 2 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 884HK UT WOS:000226075300022 ER PT J AU Polhemus, DA AF Polhemus, DA TI Further studies on the genus Orthotylus (Heteroptera : Miridae) in the Hawaiian Islands, with descriptions of thirty-four new species SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article DE plant bugs; Miridae; Orthotylus; Hawaii; new species; host plants AB Thirty-four new species in the plant bug genus Orthotylus are described from the Hawaiian Islands. The new species and their host plant associations are as follows: O. metrosideri, from Hawaii, on Metrosideros polymorpha; O. nestegiae, from Hawaii, on Nestegis sandwicensis; O. sophorae, from Hawaii, on Sophora chrysophylla; O. sophoroides, from Maui, on Sophora chrysophylla; O. perrottetiae, from Kauai, on Perrottetia sandwicensis; O. perrottetiopsis, from Maui, on Perrottetia sandwicensis; O. antidesmae, from Hawaii, on Antidesma ptayphyllum; O. melicopi, from Hawaii, on Melicope hawaiiensis; O. coprosmopsis, from Hawaii, on Coprosma menziesii; O. coprosmicola, from Molokai, on Coprosma foliosa; O. coprosmaphila, from Maui, on Coprosma montana; O. pilo, from Molokai, on Coprosma foliosa; O. hedyotiella, from Oahu, on Hedyotis acuminata; O. hedyotivorus, from Oahu, on Hedyotis terminalis; O. hedyotioides, from Maui, on Hedyotis terminalis; O. hedyotiphila, from Maui, on Hedyotis hillebrandii; O. kara, from Oahu, on Psychotria kaduana; O. kopiko, from Maui, on Psychotria mariniana; O. neopsychotriae, from Hawaii, on Psychotria hawaiiensis; O. neopsychotrioides, from Maui, on Psychotria mariniana; O. diospyropsis, from Oahu, on Diospyros hillebrandii; O. diospyricola, from Molokai, on Diospyros sandwicensis; O. diospyroides, from Maui, on Diospyros sandwicensis; O. diospyroides, from Maui, on Xylosma hawaiiense; O. xylosmicola, from Kauai, on Xylosma hawaiiense; O. clermonticola, from Maui, on Clermontia grandiflora; O. clermontioides, from Maui, on Clermontia arborescens and Clermontia kakeana; O. clermontiella, from Oahu, on Clermontia kakeana; O. pisoniopsis, from Maui, on Pisonia brunoniana; O. urericola, from Hawaii, on Urera glabra; O. ureraphila, from Maui, on Urera glabra; O. kassandroides, from Oahu, on assorted host plants; O. kassandropsis, from Maui, on assorted host plants; and O. idaida, from Oahu, on assorted host plants. Redescriptions are given for O. azalais Kirkaldy from Kauai, hypothesized to feed on Metrosideros polymorpha; and O. kassandra (Kirkaldy), from Hawaii, which occurs on assorted host plants. Distribution maps and figures of the male genitalic structures are provided for all the above species, and shaded dorsal habitus figures are provided for O. urericola and O. diospyroides. New distribution records are also provided for O. pisonioides Polhemus (with Pisonia sandwicensis documented as an additional host plant), O. pipturi Polhemus, O. coprosmae Polhemus, O. coprosmoides Polhemus, O. psychotriae Polhemus, O. psychotrioides Polhemus, and O. hedyoticola Polhemus. A revised key to Hawaiian Orthotyhts species is included, treating all species described from the archipelago to date. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Dept Entomol, MRC 105,POB 37012, Washington, DC 20013 USA. EM polhemus@si.edu NR 6 TC 8 Z9 9 U1 0 U2 3 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD WIN PY 2004 VL 112 IS 4 BP 227 EP 333 DI 10.1664/0028-7199(2004)112[0227:FSOTGO]2.0.CO;2 PG 107 WC Entomology SC Entomology GA 925CR UT WOS:000229029600003 ER PT J AU Kaeppler, AL AF Kaeppler, AL TI Appreciation and challenge: Remarks at the launch of the Oldman catalogues, 3 November 2004 SO JOURNAL OF THE POLYNESIAN SOCIETY LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU POLYNESIAN SOC INC PI AUCKLAND PA C/O MAORI STUDIES, UNIV AUCKLAND, PRIVATE BAG, AUCKLAND 92019, NEW ZEALAND SN 0032-4000 J9 J POLYNESIAN SOC JI J. Polyn. Soc. PD DEC PY 2004 VL 113 IS 4 BP 325 EP 329 PG 5 WC Anthropology SC Anthropology GA 903YR UT WOS:000227462100001 ER PT J AU Santos-Granero, F AF Santos-Granero, F TI I am Tsunki: gender and shamanism among the Shuar of Western Amazonia . SO JOURNAL OF THE ROYAL ANTHROPOLOGICAL INSTITUTE LA English DT Book Review C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL ANTHROPOLOGICAL INST PI LONDON PA 50 FITZROY STREET, LONDON W1P 5HS, ENGLAND SN 1359-0987 J9 J ROY ANTHROPOL INST JI J. R. Anthropol. Inst. PD DEC PY 2004 VL 10 IS 4 BP 939 EP 940 PG 2 WC Anthropology SC Anthropology GA 882OA UT WOS:000225947000042 ER PT J AU Altshuler, DL Dudley, R Ellington, CP AF Altshuler, DL Dudley, R Ellington, CP TI Aerodynamic forces of revolving hummingbird wings and wing models SO JOURNAL OF ZOOLOGY LA English DT Article DE aerodynamics; angle of attack; camber; hummingbird; leading edge; model wings ID HOVERING INSECT FLIGHT; LEADING-EDGE VORTEX; MECHANISMS; HAWKMOTH; ROTATION; LIFT AB A central challenge to the study of animal aerodynamics has been the measurement of forces generated by flapping wings. Relative to wings of other birds, hummingbird wings are of particular interest in that the smaller species operate in more viscous regimes (5000 < Re < 10 000) for which substantial drag and reduced lift:drag coefficients might be expected. Lift and drag forces were measured on mounted hummingbird wings and wing models spinning in continuous tipwise revolution about the wing base. Lift coefficients tended to increase as wing models became more realistic (i.e. with sharpened leading edges and with substantial camber). Lift:drag ratios of real wings were substantially higher than those of wing models, suggesting morphological contributions of feathers to lift enhancement and drag reduction. At Re = 5000, high values of the lift:drag ratio (8-16) at low angles of attack suggest that wings of hummingbirds are exceptionally good at producing lift. C1 Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Altshuler, DL (reprint author), CALTECH, Mail Code 138-78,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM doug@caltech.edu OI Altshuler, Douglas/0000-0002-1364-3617 NR 18 TC 50 Z9 51 U1 2 U2 25 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD DEC PY 2004 VL 264 BP 327 EP 332 DI 10.1017/s0952836904005813 PN 4 PG 6 WC Zoology SC Zoology GA 878TE UT WOS:000225668900001 ER PT J AU Schroll, S AF Schroll, S TI Varieties of modernism. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 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 DEC PY 2004 VL 129 IS 20 BP 115 EP 116 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 878TN UT WOS:000225669900167 ER PT J AU Hutchinson, A AF Hutchinson, A TI Animals in translation: Using the mysteries of autism to decode animal behavior. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst, Lib, Washington, DC 20560 USA. RP Hutchinson, A (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 DEC PY 2004 VL 129 IS 20 BP 154 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 878TN UT WOS:000225669900331 ER PT J AU Krot, AN Libourel, G Goodrich, CA Petaev, MI AF Krot, AN Libourel, G Goodrich, CA Petaev, MI TI Silica-rich igneous rims around magnesian chondrules in CR carbonaceous chondrites: Evidence for condensation origin from fractionated nebular gas SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SOLAR NEBULA; ISOTOPIC FRACTIONATION; REFRACTORY INCLUSIONS; SYSTEM PROCESSES; LOW-PRESSURE; EVAPORATION; RENAZZO; MELT; MATRIX; REDISTRIBUTION AB The outer portions of many type I chondrules (Fa and Fs <5 mol%) in CR chondrites (except Renazzo and Al Rais) consist of silica-rich igneous rims (SIRs). The host chondrules are often layered and have a porphyritic core surrounded by a coarse-grained igneous rim rich in low-Ca pyroxene. The SIRs are sulfide-free and consist of igneously-zoned low-Ca and high-Ca pyroxenes, glassy mesostasis, Fe, Ni-metal nodules, and a nearly pure SiO(2) phase. The high-Ca pyroxenes in these rims are enriched in Cr (up to 3.5 wt% Cr(2)O(3)) and Mn (up to 4.4 wt% MnO) and depleted in Al and Ti relative to those in the host chondrules, and contain detectable Na (up to 0.2 wt% Na(2)O). Mesostases show systematic compositional variations: Si, Na, K, and Mn contents increase, whereas Ca, Mg, Al, and Cr contents decrease from chondrule core, through pyroxene-rich igneous rim (PIR), and to SIR; FeO content remains nearly constant. Glass melt inclusions in olivine phenocrysts in the chondrule cores have high Ca and Al, and low Si, with Na, K, and Mn contents that are below electron microprobe detection limits. Fe, Ni-metal grains in SIRs are depleted in Ni and Co relative to those in the host chondrules. The presence of sulfide-free, SIRs around sulfide-free type I chondrules in CR chondrites may indicate that these chondrules formed at high (>800 K) ambient nebular temperatures and escaped remelting at lower ambient temperatures. We suggest that these rims formed either by gas-solid condensation of silica-normative materials onto chondrule surfaces and subsequent incomplete melting, or by direct SiO((gas)) condensation into chondrule melts. In either case, the condensation occurred from a fractionated, nebular gas enriched in Si, Na, K, Mn, and Cr relative to Mg. The fractionation of these lithophile elements could be due to isolation (in the chondrules) of the higher temperature condensates from reaction with the nebular gas or to evaporation-recondensation of these elements during chondrule formation. These mechanisms and the observed increase in pyroxene/olivine ratio toward the peripheries of most type I chondrules in CR, CV, and ordinary chondrites may explain the origin of olivine-rich and pyroxene-rich chondrules in general. C1 Univ Hawaii Manoa, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. CNRS, Ctr Rech Petrog & Geochim, F-54501 Vandoeuvre Les Nancy, France. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Krot, AN (reprint author), Univ Hawaii Manoa, Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu NR 66 TC 43 Z9 43 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2004 VL 39 IS 12 BP 1931 EP 1955 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 901GE UT WOS:000227270200004 ER PT J AU Dick, CW Roubik, DW Gruber, KF Bermingham, E AF Dick, CW Roubik, DW Gruber, KF Bermingham, E TI Long-distance gene flow and cross-Andean dispersal of lowland rainforest bees (Apidae : Euglossini) revealed by comparative mitochondrial DNA phylogeography SO MOLECULAR ECOLOGY LA English DT Article DE cytochrome oxidase 1; molecular clock; mtDNA; neotropical biogeography; orchid bees; tropical rainforest ID FRESH-WATER FISHES; ORCHID BEES; COSTA-RICAN; HELICONIUS BUTTERFLIES; POPULATION-STRUCTURE; MULLERIAN MIMICRY; CENTRAL-AMERICA; BIOGEOGRAPHY; SEQUENCES; HYMENOPTERA AB Euglossine bees (Apidae; Euglossini) exclusively pollinate hundreds of orchid species and comprise up to 25% of bee species richness in neotropical rainforests. As one of the first studies of comparative phylogeography in a neotropical insect group, we performed a mitochondrial DNA (mtDNA)-based analysis of 14 euglossine species represented by populations sampled across the Andes and/or across the Amazon basin. The mtDNA divergences within species were consistently low; across the 12 monophyletic species the mean intraspecific divergence among haplotypes was 0.9% (range of means, 0-1.9%). The cytochrome oxidase 1 (CO1) divergence among populations separated by the Andes (N = 11 species) averaged 1.1% (range 0.0-2.0%). The mtDNA CO1 data set displayed homogeneous rates of nucleotide substitution, permitting us to infer dispersal across the cordillera long after the final Andean uplift based on arthropod molecular clocks of 1.2-1.5% divergence per million years. Gene flow across the 3000-km breadth of the Amazon basin was inferred from identical cross-Amazon haplotypes found in five species. Although mtDNA haplotypes for 12 of the 14 euglossine species were monophyletic, a reticulate CO1 phylogeny was recovered in Euglossa cognata and E. mixta, suggesting large ancestral populations and recent speciation. Reference to closely related outgroups suggested recent speciation for the majority of species. Phylogeographical structure across a broad spatial scale is weaker in euglossine bees than in any neotropical group previously examined, and may derive from a combination of Quaternary speciation, population expansion and/or long-distance gene flow. C1 Smithsonian Trop Res Inst, APO, AA 34002 USA. Univ Minnesota, Bell Museum Nat Hist, St Paul, MN 55108 USA. RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM dickc@naos.si.edu RI Dick, Christopher/A-8744-2008 NR 68 TC 62 Z9 65 U1 1 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD DEC PY 2004 VL 13 IS 12 BP 3775 EP 3785 DI 10.1111/j.1365-294X.2004.02374.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 871RC UT WOS:000225150000013 PM 15548290 ER PT J AU Beadell, JS Gering, E Austin, J Dumbacher, JP Peirce, MA Pratt, TK Atkinson, CT Fleischer, RC AF Beadell, JS Gering, E Austin, J Dumbacher, JP Peirce, MA Pratt, TK Atkinson, CT Fleischer, RC TI Prevalence and differential host-specificity of two avian blood parasite genera in the Australo-Papuan region SO MOLECULAR ECOLOGY LA English DT Article DE Australia; avian malaria; Haemoproteus; host-specificity; Papua New Guinea; Plasmodium ID HAEMATOZOAN PARASITES; MALARIAL PARASITES; PASSERIFORM BIRDS; TURDUS-MERULA; CYTOCHROME-B; LAND BIRDS; PLASMODIUM; HEMATOZOA; PHYLOGENY; SEQUENCE AB The degree to which widespread avian blood parasites in the genera Plasmodium and Haemoproteus pose a threat to novel hosts depends in part on the degree to which they are constrained to a particular host or host family. We examined the host distribution and host-specificity of these parasites in birds from two relatively understudied and isolated locations: Australia and Papua New Guinea. Using polymerase chain reaction (PCR), we detected infection in 69 of 105 species, representing 44% of individuals surveyed (n = 428). Across host families, prevalence of Haemoproteus ranged from 13% (Acanthizidae) to 56% (Petroicidae) while prevalence of Plasmodium ranged from 3% (Petroicidae) to 47% (Ptilonorhynchidae). We recovered 78 unique mitochondrial lineages from 155 sequences. Related lineages of Haemoproteus were more likely to derive from the same host family than predicted by chance at shallow (average LogDet genetic distance = 0, n = 12, P = 0.001) and greater depths (average distance = 0.014, n = 11, P < 0.001) within the parasite phylogeny. Within two major Haemoproteus subclades identified in a maximum likelihood phylogeny, host-specificity was evident up to parasite genetic distances of 0.029 and 0.007 based on logistic regression. We found no significant host relationship among lineages of Plasmodium by any method of analysis. These results support previous evidence of strong host-family specificity in Haemoproteus and suggest that lineages of Plasmodium are more likely to form evolutionarily-stable associations with novel hosts. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. US Geol Survey, Pacific Isl Ecosyst Res Ctr, Hawaii Natl Pk, HI 96718 USA. Museum Victoria, Melbourne, Vic 3001, Australia. Calif Acad Sci, San Francisco, CA 94118 USA. MP Int Consultancy, Wokingham RG41 3AZ, Berks, England. RP Beadell, JS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM beadellj@si.edu RI Austin, Jeremy/F-8729-2010 OI Austin, Jeremy/0000-0003-4244-2942 FU NIGMS NIH HHS [1R01GM063258] NR 37 TC 118 Z9 119 U1 4 U2 33 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD DEC PY 2004 VL 13 IS 12 BP 3829 EP 3844 DI 10.1111/j.1365-294X.2004.02363.x PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 871RC UT WOS:000225150000018 PM 15548295 ER PT J AU Eggert, LS Fleischer, RC AF Eggert, LS Fleischer, RC TI Isolation of polymorphic microsatellite loci in the Hawaii amakihi (Hemignathus virens) and their use in other honeycreeper species SO MOLECULAR ECOLOGY NOTES LA English DT Article DE adaptive radiation; avian malaria; intraspecific variation AB We report the isolation and characterization of five polymorphic microsatellite loci in the Hawaii amakihi, Hemignathus virens, one of the most common native Hawaiian forest birds. These loci exhibit high levels of allelic diversity and heterozygosity in the three honeycreeper species we screened, and promise to be useful in our investigation of differences between honeycreeper populations at different elevations. C1 Smithsonian Inst, Genet Program, Natl Museum Nat Hist, Washington, DC 20008 USA. RP Eggert, LS (reprint author), Smithsonian Inst, Genet Program, Natl Museum Nat Hist, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM eggertl@nmnh.si.edu NR 9 TC 2 Z9 3 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD DEC PY 2004 VL 4 IS 4 BP 725 EP 727 DI 10.1111/j.1471-8286.2004.00793.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 876KV UT WOS:000225496600060 ER PT J AU Fabian, AC Ross, RR Miller, JM AF Fabian, AC Ross, RR Miller, JM TI On the observed disc temperature of accreting intermediate mass black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays : binaries ID X-RAY SOURCES; GALAXIES; SPECTRA; X-1; CANDIDATES; STATE AB Some ultraluminous X-ray sources in nearby galaxies show soft components resembling thermal disc emission. Calculations based on blackbody emission then indicate that the accreting black holes at the centres of these discs have masses of hundreds to thousands solar mass. Establishing the existence of such intermediate mass black holes is of considerable importance, so the assumptions and approximations lying behind blackbody spectral fits must be examined. We study here the basic assumption that the thermal emission is well-characterized by a multi-temperature blackbody spectrum. Because the opacity in the surface layers of a disc decreases at high energies, the emergent spectrum is hardened. We compute the observed spectra from discs around a non-spinning 1000-M-circle dot black hole and fit them over the XMM-Newton pn band with multicolour disc models. The typical overall spectra hardening factor usually adopted for discs around a stellar mass black hole (assuming an inclination of 60 and including relativistic effects for a non-spinning black hole) is found to be appropriate. C1 Inst Astron, Cambridge CB3 0HA, England. Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabian, AC (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM acf@ast.cam.ac.uk NR 27 TC 9 Z9 9 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2004 VL 355 IS 2 BP 359 EP 362 DI 10.1111/j.1365-2966.2004.08322.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 873FJ UT WOS:000225265000006 ER PT J AU Lazio, TJW Tarter, JC Wilner, DJ AF Lazio, TJW Tarter, JC Wilner, DJ TI The cradle of life SO NEW ASTRONOMY REVIEWS LA English DT Article ID SEARCH; GAP AB The emerging field of bioastronomy is beginning to address one of the oldest questions in science and philosophy: Are we alone? By virtue of its sheer sensitivity, high frequency coverage, and long baselines, the SKA will play a pivotal role in bioastronomical studies. It will be a unique instrument with the capability to image proto-planetary disks in nearby star-forming regions and monitor the evolution of structures within those disks ("movies of planetary formation"). It will also be able to assess the extent to which interstellar molecules are incorporated into proto-planetary disks. It will also be able to reach qualitatively new levels of sensitivity in the search for intelligence elsewhere in the Galaxy, including for the first time the realistic possibility of detecting unintentional emissions or "leakage" (such as from TV transmitters) from nearby stars. (C) 2004 Elsevier B.V. All rights reserved. C1 USN, Res Lab, Washington, DC 20375 USA. SETI Inst, Mountain View, CA 94043 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lazio, TJW (reprint author), USN, Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM Joseph.Lazio@nrl.navy.mil; tarter@vger.seti.org NR 8 TC 7 Z9 7 U1 2 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 985 EP 991 DI 10.1016/j.newar.2004.09.002 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800002 ER PT J AU Gaensler, BM Beck, R Feretti, L AF Gaensler, BM Beck, R Feretti, L TI The origin and evolution of cosmic magnetism SO NEW ASTRONOMY REVIEWS LA English DT Article ID RADIO POLARIZATION; FIELDS; GALAXIES; DEPOLARIZATION; GENERATION; SYSTEMS AB Magnetism is one of the four fundamental forces. However, the origin of magnetic fields in stars, galaxies and clusters is an open problem in astrophysics and fundamental physics. When and how were the first fields generated? Are present-day magnetic fields a result of dynamo action, or do they represent persistent primordial magnetism? What role do magnetic fields play in turbulence, cosmic ray acceleration and galaxy formation? Here, we demonstrate how the Square Kilometer Array can deliver new data which will directly address these currently unanswered issues. Much of what we present is based oil an all-sky survey of rotation measures, in which Faraday rotation towards > 10(7) background sources will provide a dense grid for probing magnetism in the Milky Way, in nearby galaxies, and in distant galaxies, clusters and protogalaxies. Using these data, we can map out the evolution of magnetised 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. With the unprecedented capabilities of the SKA, the window to the Magnetic Universe can finally be opened. (C) 2004 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. CNR, INAF, Inst Radioastron, I-40129 Bologna, Italy. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Feretti, Luigina/0000-0003-0312-6285; Gaensler, Bryan/0000-0002-3382-9558 NR 42 TC 74 Z9 74 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1003 EP 1012 DI 10.1016/j.newar.2004.09.003 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800004 ER PT J AU Rawlings, S Abdalla, FB Bridle, SL Blake, CA Baugh, CM Greenhill, LJ van der Hulst, JM AF Rawlings, S Abdalla, FB Bridle, SL Blake, CA Baugh, CM Greenhill, LJ van der Hulst, JM TI Galaxy evolution, cosmology and dark energy with the Square Kilometer Array SO NEW ASTRONOMY REVIEWS LA English DT Article ID PROBE WMAP OBSERVATIONS; LUMINOSITY FUNCTION; POWER SPECTRUM; MASS FUNCTION; SPACE; PARAMETERS; CATALOG; 2DFGRS; ORIGIN; MATTER AB The present-day Universe is seemingly dominated by dark energy and dark matter, but mapping the normal (baryonic) content remains vital for both astrophysics - understanding how galaxies form - and astro-particle physics inferring properties of the dark components. The Square Kilometer Array (SKA) will provide the only means of studying the cosmic evolution of neutral hydrogen (HI) which, alongside information on star formation from the radio continuum, is needed to understand how stars formed from gas within dark-matter over-densities and the roles of gas accretion and galaxy merging. 'All hemisphere' HI redshift surveys to z similar to 1.5 are feasible with wide-field-of-view realizations of the SKA and, by measuring the galaxy power spectrum in exquisite detail, will allow the first precise studies of the equation-of-state of dark energy. The SKA will be capable of other uniquely powerful cosmological studies including the measurement of the dark-matter power spectrum using weak gravitational lensing, and the precise measurement of H-0 using extragalactic water masers. The SKA is likely to become the premier dark-energy-measuring machine, bringing breakthroughs in cosmology beyond those likely to be made possible by combining CMB (e.g. Planck), optical (e.g. LSST, SNAP) and other early-21st-century datasets. (C) 2004 Published by Elsevier B.V. C1 Univ Oxford, Dept Phys, Oxford OX1 3RH, England. UCL, Dept Phys & Astron, London WC1E 6BT, England. Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. RP Rawlings, S (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. EM s.rawlings1@physics.ox.ac.uk RI van der Hulst, J.M./D-1857-2012; Baugh, Carlton/A-8482-2012; OI Baugh, Carlton/0000-0002-9935-9755; Abdalla, Filipe/0000-0003-2063-4345 NR 39 TC 21 Z9 21 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1013 EP 1027 DI 10.1016/j.newar.2004.09.024 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800005 ER PT J AU Greenhill, LJ AF Greenhill, LJ TI Extragalactic water masers, geometric estimation of H-0, and characterization of dark energy SO NEW ASTRONOMY REVIEWS LA English DT Article ID LARGE-MAGELLANIC-CLOUD; CEPHEID DISTANCE SCALE; TELESCOPE KEY PROJECT; METALLICITY; DISK; ANISOTROPY; GALAXY; NGC4258; PARSEC AB High precision estimation of the equation of state of dark energy depends on constraints external to analyses of Cosmic Microwave Background fluctuations. A geometric estimation of the local expansion rate, H-0, would provide the most direct and robust constraint. Traditional techniques to estimate Ho have depended on observations of standard candles for which systematic effects can be 10% or more. Observations of water maser sources in the accretion disks that feed the central engines of active galaxies enable simplified, robust, and largely geometric analyses. Many thousand maser sources will be discovered in studies with the SKA, owing to its great sensitivity. Spectroscopic monitoring and interferometric mapping - with intercontinental baselines - will allow estimation of H-0 to similar to1% and possibly better. (C) 2004 Elsevier B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM greenhill@cfa.harvard.edu NR 27 TC 12 Z9 13 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1079 EP 1084 DI 10.1016/j.newar.2004.10.002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800010 ER PT J AU Morganti, R Greenhill, LJ Peck, AB Jones, DL Henkel, C AF Morganti, R Greenhill, LJ Peck, AB Jones, DL Henkel, C TI Disks, tori, and cocoons: emission and absorption diagnostics of AGN environments SO NEW ASTRONOMY REVIEWS LA English DT Article ID ACTIVE GALACTIC NUCLEI; WATER-VAPOR MEGAMASER; H2O MASER EMISSION; PARSEC-SCALE JETS; ACCRETION DISK; NEUTRAL HYDROGEN; HI ABSORPTION; RADIO-SOURCES; BLACK-HOLES; GALAXY AB One of the most important problems in the study of active galaxies is understanding the detailed geometry, physics, and evolution of the central engines and their environments. The leading models involve an accretion disk and torus structure around a central dense object, thought to be a supermassive black hole. Gas found in the environment of active galactic nuclei (AGN) is associated with different structures: molecular accretion disks, larger scale atomic tori, ionized and neutral "cocoons" in which the nuclear regions can be embedded. All of them can be studied at radio wavelengths by various means. Here, we summarize the work that has been done to date in the radio band to characterize these structures. Much has been learned about the central few parsecs of AGN in the last few decades with contemporary instruments but the picture remains incomplete. In order to be able to define a more accurate model of this region, significant advances in sensitivity, spectral and angular resolution, and bandpass stability are required. The necessary advances will only be provided by the Square Kilometer Array and we discuss the possibilities that these dramatic improvements will open for the study of the gas in the central region of AGN. (C) 2004 Elsevier B.V. All rights reserved. C1 Netherlands Fdn Res Astron, NL-7900 AA Dwingeloo, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96720 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. MPIfR, D-53121 Bonn, Germany. RP Morganti, R (reprint author), Netherlands Fdn Res Astron, Postbus 2, NL-7900 AA Dwingeloo, Netherlands. EM morganti@astron.nl; greenhill@cfa.harvard.edu; apeck@cfa.harvard.edu; dj@sgra.jpl.nasa.gov; p220hen@m-pifr-bonn.mpg.de NR 61 TC 15 Z9 17 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1195 EP 1209 DI 10.1016/j.newar.2004.09.022 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800021 ER PT J AU Beck, R Gaensler, BM AF Beck, R Gaensler, BM TI Observations of magnetic fields in the Milky Way and in nearby galaxies with a Square Kilometre Array SO NEW ASTRONOMY REVIEWS LA English DT Article ID EXTRAGALACTIC RADIO-SOURCES; INTERSTELLAR PLASMA TURBULENCE; YOUNG SUPERNOVA-REMNANTS; ROTATION MEASURES; LARGE-SCALE; MULTIFREQUENCY POLARIMETRY; MOLECULAR CLOUDS; GALACTIC PLANE; 1.4 GHZ; MAGNETOHYDRODYNAMIC TURBULENCE AB The role of magnetic fields in the dynamical evolution of galaxies and of the interstellar medium (ISM) is not well understood, mainly because such fields are difficult to directly observe. Radio astronomy provides the best tools to measure magnetic fields: synchrotron radiation traces fields illuminated by cosmic-ray electrons, while Faraday rotation and Zeeman splitting allow us to detect fields in all kinds of astronomical plasmas, from lowest to highest densities. Here, we describe how fundamental new advances in studying magnetic fields, both in our own Milky Way and in other nearby galaxies, can be made through observations with the proposed Square Kilometre Array. Underpinning much of what we propose is an all-sky survey of Faraday rotation, in which we will accumulate tens of millions of rotation measure measurements toward background radio sources. This will provide a unique database for studying magnetic fields in individual Galactic supernova, remnants and HII regions, for characterizing the overall magnetic geometry of our Galaxy's disk and halo, and for understanding the structure and evolution of magnetic fields in galaxies. Also of considerable interest will be the mapping of diffuse polarized emission from the Milky Way in many narrow bands over a wide frequency range. This will allow us to carry out Faraday tomography of the Galaxy, yielding a high-resolution three-dimensional picture of the magnetic field within a few kpc of the Sun, and allowing us to understand its coupling to the other components of the ISM. Finally, direct synchrotron imaging of a large number of nearby galaxies, combined with Faraday rotation data, will allow us to determine the magnetic field structure in these sources, and to test both the dynamo and primordial field theories for field origin and amplification. (C) 2004 Elsevier B.V. All rights reserved. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beck, R (reprint author), Max Planck Inst Radioastron, Auf Dem Hugel 69, D-53121 Bonn, Germany. EM p181bck@mpifr-bonn.mpg.de RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 82 TC 52 Z9 52 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1289 EP 1304 DI 10.1016/j.newar.2004.09.013 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800030 ER PT J AU Wilner, DJ AF Wilner, DJ TI Imaging protoplanetary disks with a square kilometer array SO NEW ASTRONOMY REVIEWS LA English DT Article ID T-TAURI STARS; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; PLANET FORMATION; GAP FORMATION; SOLAR NEBULA; EVOLUTION; DUST; SYSTEMS AB The recent detections of extrasolar giant planets has revealed a surprising diversity of planetary system architectures, with many very unlike our Solar System. Understanding the origin of this diversity requires multi-wavelength studies of the structure and evolution of the protoplanetary disks that surround young stars. Radio astronomy and the square kilometer array (SKA) will play a unique role in these studies by imaging thermal dust emission in a representative sample of protoplanetary disks at unprecedented sub-AU scales in the innermost regions, including the "habitable zone" that lies within a few AU of the central stars. Radio observations will probe the evolution of dust grains up to centimeter-sized "pebbles", the critical first step in assembling giant planet cores and terrestrial planets, through the wavelength dependence of dust emissivity, which provides a diagnostic of particle size. High resolution images of dust emission will show directly mass concentrations and features in disk surface density related to planet building, in particular the radial gaps opened by tidal interactions between planets and disks, and spiral waves driven by embedded protoplanets. Moreover, because orbital timescales are short in the inner disk, synoptic studies over months and years will show proper motions and allow for the tracking of secular changes in disk structure. SKA imaging of protoplanetary disks will reach into the realm of rocky planets for the first time, and they will help clarify the effects of the formation of giant planets on their terrestrial counterparts. (C) 2004 Published by Elsevier B.V. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dwilner@cfa.harvard.edu NR 34 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 1387-6473 EI 1872-9630 J9 NEW ASTRON REV JI New Astron. Rev. PD DEC PY 2004 VL 48 IS 11-12 BP 1363 EP 1375 DI 10.1016/j.newar.2004.09.041 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 885HD UT WOS:000226146800037 ER PT J AU Swider, JR Walters, WB AF Swider, JR Walters, WB TI Evaluation of sensitivity and resolution enhancement in cold neutron prompt gamma-ray activation analysis using neutron lenses SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article DE prompt gamma-ray activation analysis; neutron focusing; capillary optics ID FOCUSING LENS; OPTICS; BEAMS; NIST AB Two neutron lenses were implemented in a cold neutron prompt gamma-ray activation analysis (CNPGAA) spectrometer to evaluate their enhancement of elemental sensitivity and resolution. The count rate with a lens in place was compared to the count rate of identical samples without a lens to determine the increase of sensitivity for in situ analysis. It was shown that sample sensitivities were size and shape dependent because of the Gaussian spread of neutrons at the focal spot. Samples of specific shape and size were scanned across the focused beam to examine how well element distributions could be determined from the prompt gamma-ray response. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Inst, Freer Gallery Art Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA. Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. RP Swider, JR (reprint author), Smithsonian Inst, Freer Gallery Art Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA. EM joseph.swider@asia.si.edu; ww3@umail.umd.edu NR 16 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC PY 2004 VL 226 IS 4 BP 659 EP 666 DI 10.1016/j.nimb.2004.07.015 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 875HX UT WOS:000225412100022 ER PT J AU Mangan, SA Eom, AH Adler, GH Yavitt, JB Herre, EA AF Mangan, SA Eom, AH Adler, GH Yavitt, JB Herre, EA TI Diversity of arbuscular mycorrhizal fungi across a fragmented forest in Panama: insular spore communities differ from mainland communities SO OECOLOGIA LA English DT Article DE fungal spores; species diversity; community assemblage; forest fragmentation ID TROPICAL FOREST; SPECIES-DIVERSITY; NEOTROPICAL FOREST; ROOT COLONIZATION; NEGATIVE FEEDBACK; TALLGRASS PRAIRIE; TREE DIVERSITY; SOIL PATHOGENS; PLANT; GRASSLAND AB It is now understood that alterations in the species composition of soil organisms can lead to changes in aboveground communities. In this study, we assessed the importance of spatial scale and forest size on changes in arbuscular mycorrhizal fungal (AMF) spore communities by sampling AMF spores in soils of forested mainland and island sites in the vicinity of Gatun Lake, Republic of Panama. We encountered a total of 27 AMF species or morphospecies, with 17, 8, 1 and 1 from the genera Glomus, Acaulospora, Sclerosystis, and Scutellospora, ;respectively. At small scales (< 100 m(2)), we found little evidence for spatial structuring of AMF communities ( decay of Morisita-Horn community similarity with distance). However, at large spatial scales, we found that the AMF spore community of a mainland plot was more similar to other mainland plots several kilometers (> 5) away than to nearby island plots ( within 0.7 km). Likewise, most island plots were more similar to other island plots regardless of geographic separation. There was no decay in AMF species richness ( number of species), or Shannon diversity ( number of species and their spore numbers) either with decreasing forest-fragment size, or with decreasing plant species richness. Of the six most common species that composed almost 70% of the total spore volume, spores of Glomus "tsh" and G. clavisporum were more common in soils of mainland plots, while spores of Glomus "small brown" and Acaulospora mellea were more abundant in soils of island plots. None of these common AMF species showed significant associations with soil chemistry or plant diversity. We suggest that the convergence of common species found in AMF spore communities in soils of similar forest sizes was a result of forest fragmentation. Habitat-dependent convergence of AMF spore communities may result in differential survival of tree seedlings regenerating on islands versus mainland. C1 Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. Smithsonian Trop Res Inst, Balboa 2072, Panama. Korea Natl Univ Educ, Inst Nat Sci, Chungbuck 363791, South Korea. Univ Wisconsin, Dept Biol, Oshkosh, WI 54901 USA. Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. RP Mangan, SA (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. EM smangan@indiana.edu NR 62 TC 43 Z9 48 U1 0 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD DEC PY 2004 VL 141 IS 4 BP 687 EP 700 DI 10.1007/s00442-004-1684-2 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 869QT UT WOS:000224999800014 PM 15322901 ER PT J AU Chu, X Chu, SI AF Chu, X Chu, SI TI Role of the electronic structure and multielectron responses in ionization mechanisms of diatomic molecules in intense short-pulse lasers: An all-electron ab initio study SO PHYSICAL REVIEW A LA English DT Article ID EXCHANGE-CORRELATION POTENTIALS; ABOVE-THRESHOLD IONIZATION; MULTIPHOTON IONIZATION; PHOTOELECTRON-SPECTRA; TUNNEL IONIZATION; FIELD IONIZATION; WAVE; ATOMS AB We present an all-electron ab initio study of multiphoton ionization (MPI) of diatomic molecules in intense laser pulses using the example of N-2, O-2, and F-2, and the theoretical approach of time-dependent density-functional theory with correct long-range potential. The results reveal the importance of the electronic structure and correlated multielectron responses in the ionization mechanism, and make evident inner valence electron contributions to the molecular MPI in strong laser fields. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Kansas, Dept Chem, Lawrence, KS 66045 USA. Kansas Ctr Adv Sci Comp, Lawrence, KS 66045 USA. RP Chu, X (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 25 TC 63 Z9 63 U1 1 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 2004 VL 70 IS 6 AR 061402 DI 10.1103/PhysRevA.70.061402 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 889BQ UT WOS:000226418900009 ER PT J AU Boehm, C Ascasibar, Y AF Boehm, C Ascasibar, Y TI More evidence in favor of light dark matter particles? SO PHYSICAL REVIEW D LA English DT Article ID HIGGS BOSON UNIFICATION; SUPERSYMMETRIC GUTS; CENTRAL CHARGES; SCATTERING AB In a previous work, it was found that the light dark matter scenario could be a possible explanation to the 511 keV emission line detected at the center of our galaxy. Here, we show that hints of this scenario may also have been discovered in particle physics experiments. This could explain the discrepancy between the measurement of the fine structure constant and the value referenced in the CODATA. Finally, our results indicate that some of the light dark matter features could be tested in accelerators. Their discovery might favor N=2 supersymmetry. C1 Univ Oxford, Dept Astrophys, DWB, Oxford OX1 3RH, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Univ Oxford, Dept Astrophys, DWB, 1 Keble Rd, Oxford OX1 3RH, England. EM boehm@astro.ox.ac.uk; yago@head.cfa.harvard.edu OI Ascasibar Sequeiros, Yago/0000-0003-1577-2479 NR 31 TC 29 Z9 29 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC PY 2004 VL 70 IS 11 AR 115013 DI 10.1103/PhysRevD.70.115013 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 883ZP UT WOS:000226054700087 ER PT J AU Rucinski, SM Walker, GAH Matthews, JM Kuschnig, R Shkolnik, E Marchenko, S Bohlender, DA Guenther, DB Moffat, AFJ Sasselov, D Weiss, WW AF Rucinski, SM Walker, GAH Matthews, JM Kuschnig, R Shkolnik, E Marchenko, S Bohlender, DA Guenther, DB Moffat, AFJ Sasselov, D Weiss, WW TI Differential rotation of the active G5 V star kappa(1) Ceti: Photometry from the MOST satellite SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID YOUNG SOLAR ANALOGS; LONG-TERM PHOTOMETRY; MAIN-SEQUENCE STARS; MAGNETIC ACTIVITY; STELLAR ROTATION; RADIAL-VELOCITY; AB DORADUS; EVOLUTION; TIME; SUN AB About 30.5 days of nearly uninterrupted broadband photometry of the solar-type star kappa(1) Ceti, obtained with the MOST (Microvariability and Oscillations of Stars) satellite, shows evidence for two large starspots with different rotation periods of 8.9 and similar to 9.3 days (DeltaOmega/Omega similar or equal to 4%). Ground-based measurements of Ca II H and K emission in 2002 and 2003 reveal variations in chromospheric activity with a period of about 9.3 days. The data were obtained during the MOST commissioning phase. When the data are combined with historical observations, they indicate that the 9.3 day spot has been stable in its period for over 30 yr. The photometry, with a sampling rate of approximately once per minute, was also used to search for acoustic (p-mode) oscillations in the star. We detect no clear evidence for p-modes in the kappa(1) Ceti photometry, with a noise level around 7 - 9 mumag at frequencies in the range of 0.5 - 4 mHz (3 sigma detection limit of 21 - 27 mumag). There were no flares or planetary transits during 30.5 days of MOST monitoring with light amplitudes greater than 2 mmag (durations >200 minutes) and 3 mmag (2 - 200 minute durations). While this rules out any close-in planets with Jupiter diameters greater than or equal to 0.5 and orbital inclinations close to 90degrees, the scatter in differential radial velocities permit a close giant planet in a more highly inclined orbit. C1 Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Rucinski, SM (reprint author), Univ Toronto, David Dunlap Observ, POB 360, Richmond Hill, ON L4C 4Y6, Canada. EM rucinski@astro.utoronto.ca; gordonwa@uvic.ca; matthews@astro.ubc.ca; kuschnig@astro.ubc.ca; shkolnik@astro.ubc.ca; sergey.marchenko@wku.edu; david.bohlender@nrc.ca; guenther@ap.stmarys.ca; moffat@astro.umontreal.ca; sasselov@cfa.harvard.edu; weiss@astro.univie.ac.at NR 40 TC 26 Z9 26 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2004 VL 116 IS 826 BP 1093 EP 1104 DI 10.1086/426928 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876NP UT WOS:000225504100002 ER PT J AU Price, A Gary, B Bedient, J Cook, L Templeton, M Pullen, C Starkey, D Crawford, T Corlan, R Dvorak, S Graham, K Huziak, R James, R Messier, D Quinn, N Boyd, D Blackwell, J Walker, G Mattei, M Rodriguez, D Simonsen, M Henden, A Vanmunster, T Garnavich, P Pittichova, J Matheson, T Challis, P Kirshner, RP Adams, E Harrison, T Koppelman, MD Sarty, GE Mais, DE AF Price, A Gary, B Bedient, J Cook, L Templeton, M Pullen, C Starkey, D Crawford, T Corlan, R Dvorak, S Graham, K Huziak, R James, R Messier, D Quinn, N Boyd, D Blackwell, J Walker, G Mattei, M Rodriguez, D Simonsen, M Henden, A Vanmunster, T Garnavich, P Pittichova, J Matheson, T Challis, P Kirshner, RP Adams, E Harrison, T Koppelman, MD Sarty, GE Mais, DE TI A new cataclysmic variable in Hercules SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID STANDARD STARS; SPECTROPHOTOMETRY AB We present time-series observations, spectra, and archival outburst data of a newly discovered variable star in Hercules, Var Her 04. Its orbital period, mass ratio, and outburst amplitude resemble those of the ugwz-type subclass of ugsu dwarf novae. However, its supercycle and outburst light curve defy classification as a clear ugwz. Var Her 04 is most similar to the small group of possible hydrogen-burning "period bouncers," dwarf novae that have passed beyond the period minimum and returned. C1 Amer Assoc Variable Star Observers, Clinton B Ford Astron Data & Res Ctr, Cambridge, MA 02138 USA. USN Observ, Univ Space Res Assoc, Flagstaff, AZ 86001 USA. Ctr Backyard Astrophys Belgium, B-3401 Landen, Belgium. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. Univ Saskatchewan, Saskatoon, SK S7N 5A5, Canada. Palomar Coll, Dept Astron, San Marcos, CA 92069 USA. RP Price, A (reprint author), Amer Assoc Variable Star Observers, Clinton B Ford Astron Data & Res Ctr, 25 Birch St, Cambridge, MA 02138 USA. EM aavso@aavso.org; aah@nofs.navy.mil; Tonny.Vanmunster@cbabelgium.com; pgarnavi@miranda.phys.nd.edu; jana@ifa.hawaii.edu; tmatheson@cfa.harvard.edu; pchallis@cfa.harvard.edu; rkirshner@cfa.harvard.edu; eadams@cfa.harvard.edu; tharriso@nmsu.edu; michael@aps.umn.edu; gordon.sarty@usask.ca; dmais@ligand.com OI Sarty, Gordon/0000-0001-5516-7869; Cook, Lewis/0000-0003-3332-9649 NR 15 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2004 VL 116 IS 826 BP 1117 EP 1122 DI 10.1086/427272 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 876NP UT WOS:000225504100005 ER PT J AU Cairns, SD AF Cairns, SD TI The azooxanthellate Scleractinia (Coelenterata : Anthozoa) of Australia SO RECORDS OF THE AUSTRALIAN MUSEUM LA English DT Review ID CORALS SCLERACTINIA; CNIDARIA ANTHOZOA; ASCOTHORACIDA; CRUSTACEA; ISLANDS; VANUATU; FOSSIL; GENUS AB A total of 237 species of azooxanthellate Scleractinia are reported for the Australian region, including seamounts off the eastern coast. Two new genera (Lissotrochus and Stolarskicyathus) and 15 new species are described: Crispatotrochus gregarius, Paracyathus darwinensis, Stephanocyathus imperialis, Trochocyathus wellsi, Conocyathus formosus, Dunocyathus wallaceae, Foveolocyathus parkeri, Idiotrochus alatus, Lissotrochus curvatus, Sphenotrochus cuneolus, Placotrochides cylindrica, P. minuta, Stolarskicyathus pocilliformis, Balanophyllia spongiosa, and Notophyllia hecki. Also, one new combination is proposed: Petrophyllia rediviva. Each species account includes an annotated synonymy for all Australian records as well as reference to extralimital accounts of significance, the type locality, and deposition of the type. Tabular keys are provided for the Australian species of Culicia and all species of Conocyathus and Placotrochides. A discussion of previous studies of Australian azooxanthellate corals is given in narrative and tabular form. This study was based on approximately 5500 previously unreported specimens collected from 500 localities, as well as a re-examination of most of the types and previously reported specimens from the Australian region. Fifty-six species are recorded as new to Australia; 183 state range extensions are listed; and 96 worldwide bathymetric range extensions are noted. In order to characterize the Australian fauna, all 703 known azooxanthellate species were tabulated as to coloniality, method of attachment, and depth range: 187 species are colonial, 516 solitary; 373 are attached, 265 free, and 54 transversely dividing; and 2001000 in is the most common depth range. Compared to all azooxanthellate species, those from Australia have a slightly higher percentage of species that are solitary and unattached (or transversely dividing), due to a disproportionate number of species in the families Flabellidae and Turbinoliidae. Bathymetrically they are typical of the worldwide fauna. Sixty-seven species are endemic to the Australian region. Both UPGMA cluster analysis and MDS ordination reveal two main regions: a northern tropical region and a southern warm temperate region, consistent with zonation patterns of shallow-water marine invertebrates. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM cairns.stephen@nmnh.si.edu NR 180 TC 19 Z9 22 U1 1 U2 1 PU AUSTRALIAN MUSEUM PI SYDNEY PA 6 COLLEGE ST, SYDNEY, NSW 2010, AUSTRALIA SN 0067-1975 J9 REC AUST MUS JI Rec. Aust. Mus. PD DEC 1 PY 2004 VL 56 IS 3 BP 259 EP 329 PG 71 WC Zoology SC Zoology GA 879RM UT WOS:000225735000001 ER PT J AU Bednarski, M Morales-Ramirez, A AF Bednarski, M Morales-Ramirez, A TI Composition, abundance and distribution of macrozooplankton in Culebra Bay, Gulf of Papagayo, Pacific coast of Costa Rica and its value as bioindicator of pollution SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE macrozooplankton; pollution; Eastern Pacific; MDS; microcrustacean; Culebra bay; Costa Rica ID ZOOPLANKTON POPULATIONS; KINGSTON HARBOR; COPEPODS; FLUCTUATIONS; MANAGEMENT; JAMAICA; OUTFLOW; FISH AB The abundance. distribution and composition of the macrozooplankton of Culebra Bay, Costa Rica (10degrees38'N - 85degrees40'W) were studied at four stations throughout the dry (February - May) and rainy (September - November) seasons of 2000. The samples were collected at two-week intervals using a 500mum mesh net with a 0.5 m diameter opening. Copepods (23-31%) and ostracods (20-34%) were predominant throughout the x-ear, followed by cladocerans (2.5-14%), zoea (6.6-9.5%). and siphonophores; (2.5-7.2%). High densities of zooplankton were obtained in February and March with peak abundance on March IS. The lowest densities were observed on September 3 and November 5. Significant differences in abundances at each station were observed for the groups Acartia tonsa (Copepoda), Ctenophora, Medusae, Ostracoda. Zoea, and Amphipoda. Comparison of the dry and rainy seasons revealed significantly higher zooplankton abundance in the dry season and copepod domination of all stations; during the rainy season ostracods dominated the off-shore areas. Zooplankion abundance and distribution are influenced by upwelling, which occurs during the dry season in Culebra Bay. C1 Ctr Trop Marine Ecol, ZMT, D-28359 Bremen, Germany. Univ Costa Rica, Escuela Biol, Ctr Invest Ciencias Mar & Limnol, CIMAR, San Pedro 2060, Costa Rica. RP Bednarski, M (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM bednarskim@si.edu; amorales@cariari.ucr.ac.cr NR 32 TC 11 Z9 12 U1 0 U2 0 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA RICA SN 0034-7744 EI 2215-2075 J9 REV BIOL TROP JI Rev. Biol. Trop. PD DEC PY 2004 VL 52 SU 2 BP 105 EP 119 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 893LA UT WOS:000226719300011 PM 17465134 ER PT J AU Goodyear, AC AF Goodyear, AC TI Gyorgy Kepes, Billy Kluver, and American art of the 1960s: Defining attitudes toward science and technology SO SCIENCE IN CONTEXT LA English DT Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Goodyear, AC (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 104 TC 7 Z9 7 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0269-8897 J9 SCI CONTEXT JI Sci. Context PD DEC PY 2004 VL 17 IS 4 BP 611 EP 635 DI 10.1017/S0269889704000286 PG 25 WC History & Philosophy Of Science SC History & Philosophy of Science GA 899CV UT WOS:000227123400007 ER PT J AU Murdoch, JD Ralls, K Cypher, BL AF Murdoch, JD Ralls, K Cypher, BL TI Two observations of tree climbing by the San Joaquin kit fox SO SOUTHWESTERN NATURALIST LA English DT Article ID FOOD AB Tree climbing behavior is rarely observed among the Canidae and has not been observed in kit foxes (Vulpes macrotis). While conducting another behavioral study in Bakersfield, California in November 2002, we observed kit foxes climb trees on 2 occasions. Our observations demonstrate that kit foxes are capable of climbing trees and of agile mobility among tree branches. Our observations also provide an example of the behavioral plasticity of kit foxes, a characteristic that might contribute to their ability to successfully inhabit anthropogenically altered environments. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Endangered Species Recovery Program, Bakersfield, CA 93309 USA. Univ Denver, Dept Biol, Denver, CO 80208 USA. RP Murdoch, JD (reprint author), Univ Oxford, Wildlife Conservat Res Unit, Tubney OX13 5QL, Oxon, England. EM james.murdoch@zoology.ox.ac.uk NR 10 TC 0 Z9 0 U1 2 U2 4 PU SOUTHWESTERN ASSN NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 J9 SOUTHWEST NAT JI Southw. Natural. PD DEC PY 2004 VL 49 IS 4 BP 522 EP 523 DI 10.1894/0038-4909(2004)049<0522:TOOTCB>2.0.CO;2 PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 887XC UT WOS:000226337800017 ER PT J AU DeLuca, WV Studds, CE Rockwood, LL Marra, PP AF DeLuca, WV Studds, CE Rockwood, LL Marra, PP TI Influence of land use on the integrity of marsh bird communities of Chesapeake Bay, USA SO WETLANDS LA English DT Article DE threshold response; specialist; generalist; index of marsh bird community integrity; estuarine wetlands; Chesapeake Bay ID BIOTIC INTEGRITY; BIOLOGICAL INTEGRITY; ECOLOGICAL CONDITION; SPECIES RICHNESS; URBAN GRADIENT; WATER-QUALITY; INDICATORS; HABITAT; INDEX; RIVER AB The landscape within the Chesapeake Bay watershed has been and continues to be impacted by human modifications. Understanding if such anthropogenic disturbances influence organisms that are dependent upon estuarine wetlands remains unclear. We developed an index of marsh bird community integrity (IMBCI) to evaluate marsh bird communities and wetland condition. During the 2002 and 2003 summers, we detected 30 bird species at 219 point count locations distributed among 96 wetlands. lMBCI scores for each wetland were used to determine whether wetland habitat characteristics and urban/suburban development, agriculture, and forest at three different spatial scales (watershed, 1000-m buffer, and 500-m buffer) influenced marsh bird community integrity. We found no relationship between lMBCI scores and wetland habitat characteristics, implying that marsh bird community integrity is not related to any single plant community. Nonparametric changepoint analysis indicated that marsh bird community integrity was significantly reduced when the amount of urban/suburban development within 500 m and 1000 m of the marsh exceeded 14% and 25%, respectively. There was no effect of urban/suburban development on lMBCI scores at the watershed scale. The results of our study demonstrate that marsh bird community integrity shows a threshold response to urban/suburban development at local scales. lMBCI scores, combined with the identification of a land-use threshold, can be easy to interpret and may help communicate complex ecological data to natural resource managers and conservation planners. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP DeLuca, WV (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM delucaw@si.edu RI Studds, Colin/C-3701-2012 NR 60 TC 47 Z9 54 U1 5 U2 30 PU SOC WETLAND SCIENTISTS PI LAWRENCE PA 810 E TENTH ST, P O BOX 1897, LAWRENCE, KS 66044 USA SN 0277-5212 J9 WETLANDS JI Wetlands PD DEC PY 2004 VL 24 IS 4 BP 837 EP 847 DI 10.1672/0277-5212(2004)024[0837:IOLUOT]2.0.CO;2 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 886WW UT WOS:000226264700013 ER PT J AU Jehl, JR AF Jehl, JR TI Foraging by a Red-Tailed Hawk along a wetland edge: How large a duck can be captured? SO WILSON BULLETIN LA English DT Article AB A Red-tailed Hawk (Buteo jamaicensis; estimated mass 1,000-1,200 g) failed to kill a Red-breasted Merganser (Mergus serrator; estimated mass 1,150 g) that it captured in shallow water (<25 cm), but evidently dispatched a starving Red-necked Grebe (Podiceps grisegena; mass 645-660 g). These observations are pertinent to estimating the upper mass limit for successful foraging in water. C1 US Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. Hawk Mt Sanctuary, Acopian Ctr, Orwigsburg, PA 17961 USA. RP Jehl, JR (reprint author), 2752 Poplar Ln, Annapolis, MD 21401 USA. EM grebe5k@cs.com NR 17 TC 1 Z9 1 U1 1 U2 4 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 USA SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD DEC PY 2004 VL 116 IS 4 BP 354 EP 356 DI 10.1676/04-040 PG 3 WC Ornithology SC Zoology GA 898TY UT WOS:000227100300012 ER PT J AU Bradley, B Stanford, D AF Bradley, B Stanford, D TI The North Atlantic ice-edge corridor: a possible Palaeolithic route to the New World SO WORLD ARCHAEOLOGY LA English DT Article DE clovis; pre-clovis; solutrean; colonization of New World; Paleoindian; ice-edge corridor ID BRITISH-COLUMBIA; FLUTED POINT; AMERICA; ARCHAEOLOGY; SITE; SETTLEMENT; CANADA; HUMANS; SHELL AB The early peopling of the New World has been a topic of intense research since the early twentieth century. We contend that the exclusive focus of research on a Beringian entry point has not been productive. Evidence has accumulated over the past two decades indicating that the earliest origin of people in North America may have been from south-western Europe during the last glacial maximum. In this summary we outline a theory of a Solutrean origin for Clovis culture and briefly present the archaeological data supporting this assertion. C1 Univ Exeter, Exeter EX4 4QJ, Devon, England. Smithsonian Inst, Natl Museum Natl Hist, Washington, DC 20560 USA. RP Bradley, B (reprint author), Univ Exeter, Exeter EX4 4QJ, Devon, England. NR 74 TC 57 Z9 60 U1 4 U2 24 PU ROUTLEDGE TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0043-8243 J9 WORLD ARCHAEOL JI World Archaeol. PD DEC PY 2004 VL 36 IS 4 BP 459 EP 478 DI 10.1080/0043824042000303656 PG 20 WC Archaeology SC Archaeology GA 883MG UT WOS:000226015900003 ER PT J AU Vrinceanu, D Sadeghpour, HR Bartschat, K AF Vrinceanu, D Sadeghpour, HR Bartschat, K TI Electron-impact broadening of Sr+ lines in ultracold neutral plasmas SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID SCATTERING; SHIFT AB We report on calculations of electron-impact broadening of Sr+ spectral lines in ultracold neutral plasmas. Optical absorption imaging of an ultracold Sr plasma has recently been used to infer detailed in situ information on the ion dynamics. We modify our recent treatment of collisional broadening in He metastable lines to the collision of electrons from Sr+ ions. The required scattering matrix elements are obtained from an ab initio R-matrix calculation. C1 ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP ITAMP, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM dvrinceanu@cfa.harvard.edu RI Bartschat, Klaus/I-2527-2012 NR 17 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD NOV 28 PY 2004 VL 37 IS 22 BP L371 EP L375 DI 10.1088/0953-4075/37/22/l02 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 879MM UT WOS:000225721900002 ER PT J AU Fonseca, DM Keyghobadi, N Malcolm, CA Schaffner, F Mogi, M Fleischer, RC Wilkerson, RC AF Fonseca, DM Keyghobadi, N Malcolm, CA Schaffner, F Mogi, M Fleischer, RC Wilkerson, RC TI Outbreak of West Nile virus in North America - Response SO SCIENCE LA English DT Letter ID HOST-FEEDING PATTERNS; MOSQUITOS; CULICIDAE; DIPTERA; BIRDS C1 Acad Nat Sci Philadelphia, Philadelphia, PA 19103 USA. Okanagan Univ Coll, Kelowna, BC V1V 1V7, Canada. Univ London Queen Mary & Westfield Coll, Sch Biol Sci, London E1 4NS, England. Adege, EID Mediterranee, F-34184 Montpellier 4, France. Saga Med Sch, Saga 8498501, Japan. Smithsonian Inst, Genet Program, Washington, DC 20008 USA. Walter Reed Army Inst Res, Silver Spring, MD 20910 USA. RP Fonseca, DM (reprint author), Acad Nat Sci Philadelphia, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. OI Fonseca, Dina/0000-0003-4726-7100 NR 15 TC 4 Z9 5 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD NOV 26 PY 2004 VL 306 IS 5701 BP 1473 EP 1475 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 875ST UT WOS:000225442700021 ER PT J AU Bush, MB De Oliveira, PE Colinvaux, PA Miller, MC Moreno, JE AF Bush, MB De Oliveira, PE Colinvaux, PA Miller, MC Moreno, JE TI Amazonian paleoecological histories: one hill, three watersheds SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE fossil pollen; cation; climate history; cooling; ice age; insolation; Milankovitch; lake-level; Pleistocene; precession; South America ID LAST GLACIAL MAXIMUM; MODERN POLLEN RAIN; LATE QUATERNARY; ATMOSPHERIC CO2; SOUTH-AMERICA; LOWLAND AMAZONIA; LATE PLEISTOCENE; NORTH-AMERICA; CLIMATE; FOREST AB Data from the Hill of Six Lakes, in the northwestern Brazilian Amazon region, provide three records of paleoclimatic and vegetation change in lowland Amazonia that span the last 170,000 years. Three lakes, Verde, Pata and Dragdo, which occupy separate watersheds on the hill, provide the most detailed image yet obtained of ice-age conditions in lowland Amazonia. Well-dated sedimentary records for fossil palynological, charcoal, cation, and pigment, data are presented. The data indicate the continuous presence of mesic forest throughout the last ice age. Oscillations of lake level are recorded and the lowstands are attributed to reduced precipitation inputs to systems delicately balanced between water loss (leakage through the floor of the basin) and gain (precipitation). Gross stratigraphy, algal remains, and paleochemistry suggest that the stands of high and low lake level were cyclic, apparently correlating precessional orbital variation. Times of lake lowstand coincide with wet season (December January February, DJF) insolation minima. The strongest of eight lowstand cycles occurred ca. 35,000 to 27,000 cal BP. Even during lowstand episodes, pollen is well preserved and provides a clear signal of uninterrupted forest cover. The principal lowland elements are continuously present in the record, suggesting the long-term (Quaternary) availability of the lowland forest biome in this region. However, during the late Pleistocene the forest changed in composition with the expansion or invasion of montane floral elements creating communities of the mesic forest biome without modem analogs. While precipitation cycles were causing lake levels to rise and fall, the principal influence on vegetation appears to have been cooling. In the late Pleistocene, the population expansion of montane elements at lower elevations is consistent with a cooling of 4-5degreesC. (C) 2004 Elsevier B.V. All rights reserved. C1 Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. Univ Guarulhos, Lab Geociencias, BR-07023070 Sao Paulo, Brazil. Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. Marine Biol Lab, Woods Hole, MA 02543 USA. Univ Cincinnati, Dept Biol Sci, Cincinnati, OH 54221 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Bush, MB (reprint author), Florida Inst Technol, Dept Biol Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM mbush@fit.edu RI De Oliveira, Paulo/B-4559-2017; OI De Oliveira, Paulo/0000-0003-1040-4001; Bush, Mark/0000-0001-6894-8613 NR 98 TC 85 Z9 88 U1 2 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD NOV 25 PY 2004 VL 214 IS 4 BP 359 EP 393 DI 10.1016/j.palaeo.2004.07.031 PG 35 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 874KN UT WOS:000225349400005 ER PT J AU Voigt, O Collins, AG Pearse, VB Pearse, JS Ender, A Hadrys, H Schierwater, B AF Voigt, O Collins, AG Pearse, VB Pearse, JS Ender, A Hadrys, H Schierwater, B TI Placozoa - no longer a phylum of one SO CURRENT BIOLOGY LA English DT Letter ID TRICHOPLAX-ADHAERENS; METAZOAN EVOLUTION; PHYLOGENY C1 Inst Anim Ecol & Cell Biol, Div Ecol & Evolut, D-30559 Hannover, Germany. Univ Erlangen Nurnberg, Dept Mol Plant Physiol, D-91058 Erlangen, Germany. Smithsonian Inst, Natl Museum Amer Hist, Natl Systemat Lab, NMFS, Washington, DC 20013 USA. Univ Calif Santa Cruz, Long Marine Lab, Santa Cruz, CA 95060 USA. Katharinen Hosp, Zent Inst Transfus Med & Blutspendedienst, D-70174 Stuttgart, Germany. RP Voigt, O (reprint author), Inst Anim Ecol & Cell Biol, Div Ecol & Evolut, Bunteweg 17D, D-30559 Hannover, Germany. EM CollinsA@Sl.edu RI Collins, Allen/A-7944-2008; Voigt, Oliver/A-7449-2011 OI Collins, Allen/0000-0002-3664-9691; Voigt, Oliver/0000-0001-8708-0872 NR 12 TC 56 Z9 56 U1 0 U2 7 PU CELL PRESS PI CAMBRIDGE PA 1100 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD NOV 23 PY 2004 VL 14 IS 22 BP R944 EP R945 DI 10.1016/j.cub.2004.10.036 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 874LV UT WOS:000225352800006 PM 15556848 ER PT J AU Iono, D Yun, MS Mihos, JC AF Iono, D Yun, MS Mihos, JC TI Radial gas flows in colliding galaxies: Connecting simulations and observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (UGC 12914/12915); galaxies : interactions; galaxies : kinematics and dynamics; methods : numerical ID INTERACTING DISK GALAXIES; ON SPIRAL GALAXIES; MOLECULAR GAS; BARRED GALAXIES; ROTATION CURVES; STAR-FORMATION; INFRARED GALAXIES; DISTANT GALAXIES; MERGING GALAXIES; CHAIN GALAXIES AB We investigate the detailed response of gas to the formation of transient and long-lived dynamical structures induced in the early stages of a disk-disk collision and identify observational signatures of radial gas inflow through a detailed examination of the collision simulation of an equal-mass bulge-dominated galaxy. Our analysis and discussion mainly focuses on the evolution of the diffuse and dense gas in the early stages of the collision, when the two disks are interacting but have not yet merged. Stars respond to the tidal interaction by forming both transient arms and long-lived m = 2 bars, but the gas response is more transient, flowing directly toward the central regions within about 10(8) yr after the initial collision. The rate of inflow declines when more than half of the total gas supply reaches the inner few kiloparsecs, where the gas forms a dense nuclear ring inside the stellar bar. The average gas inflow rate to the central 1.8 kpc is similar to 7 M-. yr(-1) with a peak rate of 17 M-. yr(-1). Gas with high volume density is found in the inner parts of the postcollision disks at size scales close to the spatial resolution of the simulations, and this may be a direct result of shocks traced by the discontinuity in the gas velocity field. The evolution of gas in a bulgeless progenitor galaxy is also discussed, and a possible link to the "chain galaxy'' population observed at high redshifts is inferred. The evolution of the structural parameters such as asymmetry and concentration of both stars and gas are studied in detail. Further, a new structure parameter ( the compactness parameter K) that traces the evolution of the size scale of the gas relative to the stellar disk is introduced, and this may be a useful tracer to determine the merger chronology of colliding systems. Noncircular gas kinematics driven by the perturbation of the nonaxisymmetric structure can produce distinct emission features in the "forbidden velocity quadrants'' of the position-velocity diagram (PVD). The dynamical mass calculated using the rotation curve derived from fitting the emission envelope of the PVD can determine the true mass to within 20% - 40%. The evolution of the molecular fraction (M-H2/MH2+H I) is a potential tracer to quantitatively assign the age of the interaction, but the application to real systems may require additional observational diagnostics to properly assess the exact chronology of the merger evolution. C1 Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. RP Iono, D (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. OI Mihos, Chris/0000-0002-7089-8616 NR 89 TC 47 Z9 47 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 NOV 20 PY 2004 VL 616 IS 1 BP 199 EP 220 DI 10.1086/424797 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872HY UT WOS:000225199500017 ER PT J AU Burkert, A Hartmann, L AF Burkert, A Hartmann, L TI Collapse and fragmentation in finite sheets SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : structure; stars : formation ID ELONGATED CYLINDRICAL CLOUDS; INITIAL MASS FUNCTION; ORION NEBULA CLUSTER; MOLECULAR CLOUD; STAR-FORMATION; STELLAR CLUSTERS; GRAVITATIONAL COLLAPSE; INTERSTELLAR-MEDIUM; MAGNETIZED CLOUDS; TURBULENT MODEL AB We present two-dimensional simulations of finite, self-gravitating gaseous sheets. Unlike the case of infinite sheets, such configurations do not constitute equilibrium states but instead are subject to global collapse unless countered by pressure forces or rotation. The initial effect of finite geometry is to promote concentrations of material at the edges of the sheet. If the sheet is not perfectly circular, gravitational focusing results in enhanced concentrations of mass. In the second-most simple geometry, that of an elliptical outer boundary, the general result is collapse to a filamentary structure with the densest concentrations of mass at the ends of the filament. We suggest that these simple calculations have interesting implications for the gravitational evolution of overall molecular cloud structure, envisioning that such clouds might originate as roughly sheetlike sections of gas accumulated as a result of large-scale flows in the local interstellar medium. We show some examples of local clouds with overall filamentary shape and denser concentrations of mass and star clusters near the ends of the overall extended structure, suggestive of our simple ellipse collapse calculations. We suggest that cluster-forming gas is often concentrated as a result of gravity acting on irregular boundaries; this mechanism can result in very rapid infall of gas, which may be of importance to the formation of massive stars. This picture suggests that much of the supersonic "turbulence'' observed in molecular clouds might be gravitationally generated. Our results may provide impetus for further theoretical explorations of global gravitational effects in molecular clouds and their implications for generating the substructure needed for fragmentation into stars and clusters. C1 Univ Observ Munich, D-81679 Munich, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burkert, A (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM burkert@usm.uni-muenchen.de; hartmann@cfa.harvard.edu NR 59 TC 108 Z9 108 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 NOV 20 PY 2004 VL 616 IS 1 BP 288 EP 300 DI 10.1086/424895 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872HY UT WOS:000225199500024 ER PT J AU Orosz, JA McClintock, JE Remillard, RA Corbel, S AF Orosz, JA McClintock, JE Remillard, RA Corbel, S TI Orbital parameters for the black hole binary XTE J1650-500 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; black hole physics; stars : individual (XTE J1650-500); X-rays : binaries; X-rays : stars ID QUASI-PERIODIC OSCILLATIONS; DYNAMICAL EVIDENCE; STELLAR PHOTOMETRY; GRO J1655-40; MASS; STAR; CANDIDATE; CURVE; SPECTROSCOPY; J0422+32 AB We present R-band photometry of the X-ray transient and candidate black hole binary XTE J1650-500 obtained between 2003 May and August with the 6.5 m Clay telescope. A timing analysis of these data reveals a photometric period of 0.3205+/-0.0007 days (i.e., 7.63 hr) with a possible alias at 0.3785 days (9.12 hr). Our photometry completely rules out the previously published spectroscopic period of 0.212 days (5.09 hr). Consequently, we reanalyzed the 15 archival ESO VLT spectra (obtained 2002 June by Sanchez-Fernandez et al.) that were the basis of the previously published spectroscopic period. We used a "rest-frame search'' technique that is well suited for cases in which the signal-to-noise ratio of individual spectra is low. For each of roughly 1.1 million binary ephemerides, we summed all of the spectra in a trial rest frame of the secondary star, and each rest-frame spectrum was cross-correlated against a template spectrum. We then searched for the set of orbital parameters that produced the strongest cross-correlation value. The results confirmed the photometric period of 0.3205 days and ruled out the alias period near 0.38 days. The best value for the velocity semiamplitude of the companion star is K-2=435+/-30 km s(-1), and the corresponding optical mass function is f (M)=2.73+/-0.56 M-circle dot. The spectral type of the companion star is not well constrained because we only have six template spectra available to us. The K4 V template provides the best match; next-best matches are provided by the G5 V and K2 III templates. We also find that the accretion disk dominates the light in the R band where the disk fraction is 80% or higher, although this value should be treated with caution owing to the poor signal-to-noise ratio and the limited number of templates. The amplitude of the phased R-band light curve is 0.2 mag, which gives a lower limit to the inclination of 50degrees+/-3degrees in the limiting case of no contribution to the R-band light curve from the accretion disk. If the mass ratio of XTE J1650-500 is similar to the mass ratios of other black hole binaries, such as A0620-00 or GRS 1124-683 (e.g., Qgreater than or similar to10), then our lower limit to the inclination gives an upper limit to the mass of the black hole in XTE J1650-500 of M(1)less than or similar to7.3 Mcircle dot. However, the mass can be considerably lower if the R-band flux is dominated by the accretion disk. For example, if the accretion disk does contribute 80% of the flux, as our preliminary results suggest, then the black hole mass would be only about 4 M-circle dot. C1 San Diego State Univ, Dept Astron, San Diego, CA 82182 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. CEA Saclay, Serv Astrophys, DAPNIA, F-91191 Gif Sur Yvette, France. Univ Paris 07, F-75251 Paris 5, France. RP San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 82182 USA. EM orosz@sciences.sdsu.edu; jem@cfa.harvard.edu; rr@space.mit.edu; corbel@discovery.saclay.cea.fr NR 56 TC 67 Z9 67 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 NOV 20 PY 2004 VL 616 IS 1 BP 376 EP 382 DI 10.1086/424892 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872HY UT WOS:000225199500032 ER PT J AU Gaensler, BM van der Swaluw, E Camilo, F Kaspi, VM Baganoff, FK Yusef-Zadeh, F Manchester, RN AF Gaensler, BM van der Swaluw, E Camilo, F Kaspi, VM Baganoff, FK Yusef-Zadeh, F Manchester, RN TI The mouse that soared: High-resolution X-ray imaging of the pulsar-powered bow shock G359.23-0.82 SO ASTROPHYSICAL JOURNAL LA English DT Review DE ISM : individual (G359.23-0.82); pulsars : individual (PSR J1747-2958); stars : neutron; stars : winds, outflows ID SUPERNOVA REMNANT W44; LOCAL INTERSTELLAR-MEDIUM; GALACTIC-CENTER REGION; YOUNG RADIO PULSAR; CRAB-NEBULA; WIND NEBULA; MILLISECOND PULSAR; SYNCHROTRON NEBULA; VELA PULSAR; MAGNETIC-FIELD AB We present an observation with the Chandra X-Ray Observatory of the unusual radio source G359.23-0.82 ("the Mouse''), along with updated radio timing data from the Parkes radio telescope on the coincident young pulsar J1747-2958. We find that G359.23-0.82 is a very luminous X-ray source [L-X(0.5-8.0 keV)=5x10(34) ergs s(-1) for a distance of 5 kpc] whose morphology consists of a bright head coincident with PSR J1747-2958 plus a 45" long narrow tail whose power-law spectrum steepens with distance from the pulsar. We thus confirm that G359.23-0.82 is a bow shock pulsar wind nebula powered by PSR J1747-2958; the nebular standoff distance implies that the pulsar is moving with a Mach number of similar to60, suggesting a space velocity approximate to600 km s(-1) through gas of density approximate to0.3 cm(-3). We combine the theory of ion-dominated pulsar winds with hydrodynamic simulations of pulsar bow shocks to show that a bright elongated X-ray and radio feature extending 10" behind the pulsar represents the surface of the wind termination shock. The X-ray and radio "trails'' seen in other pulsar bow shocks may similarly represent the surface of the termination shock, rather than particles in the postshock flow as is usually argued. The tail of the Mouse contains two components: a relatively broad region seen only at radio wavelengths, and a narrow region seen in both radio and X-rays. We propose that the former represents material flowing from the wind shock ahead of the pulsar's motion, while the latter corresponds to more weakly magnetized material streaming from the backward termination shock. This study represents the first consistent attempt to apply our understanding of "Crab-like'' nebulae to the growing group of bow shocks around high-velocity pulsars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. FOM Inst Plasma Phys, NL-3430 BE Nieuwegein, Netherlands. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA. EM bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 104 TC 99 Z9 99 U1 1 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 NOV 20 PY 2004 VL 616 IS 1 BP 383 EP 402 DI 10.1086/424906 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872HY UT WOS:000225199500033 ER PT J AU Slane, P Helfand, DJ van der Swaluw, E Murray, SS AF Slane, P Helfand, DJ van der Swaluw, E Murray, SS TI New constraints on the structure and evolution of the pulsar wind nebula 3C 58 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (3C 58); pulsars : individual (PSR J0205+6449); stars : neutron; supernova remnants; X-rays : general ID SUPERNOVA REMNANT 3C-58; X-RAY-SPECTRUM; 3C 58; NEUTRON-STAR; CHANDRA OBSERVATIONS; CRAB-NEBULA; DISCOVERY; RADIO; EMISSION; INSTABILITY AB We present an investigation of the spectral and spatial structure of the X-ray emission from 3C 58 based on a 350 ks observation with the Chandra X-ray Observatory. This deep image, obtained as part of the Chandra Large Project program, reveals new information on nearly all spatial scales in the pulsar wind nebula (PWN). On the smallest scales, we derive an improved limit of T<1.02x10(6) K for blackbody emission from the entire surface of the central neutron star (NS), confirming the need for rapid, nonstandard cooling in the stellar interior. Furthermore, we show that the data are consistent with emission from a light-element atmosphere with a similar temperature. Surrounding the NS, a toroidal structure with a jet is resolved, consistent with earlier measurements and indicative of an east-west orientation for the projected rotation axis of the pulsar. A complex of looplike X-ray filaments fills the nebula interior and corresponds well with structures seen in the radio band. Several of the structures coincide with optical filaments as well. The emission from the interior of the PWN, including the pulsar, jet, and filaments, is primarily nonthermal in nature. The power-law index steepens with radius, but appears to also show small azimuthal variations. The outermost regions of the nebula require a thermal emission component, confirming the presence of an ejecta-rich swept up shell. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. FOM Inst Plasma Phys Rijnhuizen, NL-3430 BE Nieuwegein, Netherlands. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 83 Z9 83 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 NOV 20 PY 2004 VL 616 IS 1 BP 403 EP 413 DI 10.1086/424814 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872HY UT WOS:000225199500034 ER PT J AU Battat, JB Blundell, R Moran, JM Paine, S AF Battat, JB Blundell, R Moran, JM Paine, S TI Atmospheric phase correction using total power radiometry at the submillimeter array SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; instrumentation : adaptive optics; site testing; submillimeter; techniques : interferometric ID PRECIPITABLE WATER-VAPOR; MILLIMETER INTERFEROMETRY; MICROWAVE RADIOMETER; 22 GHZ; FLUCTUATIONS; TROPOSPHERE; CALIBRATION; SPECTRUM; MONITORS; LIQUID AB Phase noise caused by an inhomogeneous, time-variable water vapor distribution in our atmosphere reduces the angular resolution, visibility amplitude, and coherence time of millimeter and submillimeter wavelength interferometers. We present early results from our total power radiometry phase correction experiment carried out with the Submillimeter Array on Mauna Kea. From accurate measurements of the atmospheric emission along the lines of sight of two elements of the array, we estimated the differential atmospheric electrical path between them. In one test, presented here, the phase correction technique reduced the rms phase noise at 230 GHz from 72degrees to 27degrees over a 20 minute period with a 2.5 s integration time. This corresponds to a residual differential electrical path of 98 mm, or 15 mm of precipitable water vapor, and raises the coherence in the 20 minute period from 0.45 to 0.9. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Battat, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-10, Cambridge, MA 02138 USA. EM jbattat@cfa.harvard.edu OI Paine, Scott/0000-0003-4622-5857; Moran, James/0000-0002-3882-4414 NR 23 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2004 VL 616 IS 1 BP L71 EP L74 DI 10.1086/423932 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800018 ER PT J AU Beuther, H Zhang, Q Hunter, TR Sridharan, TK Zhao, JH Sollins, P Ho, PTP Liu, SY Ohashi, N Su, YN Lim, J AF Beuther, H Zhang, Q Hunter, TR Sridharan, TK Zhao, JH Sollins, P Ho, PTP Liu, SY Ohashi, N Su, YN Lim, J TI Submillimeter Array multiline observations of the massive star-forming region IRAS 18089-1732 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; line : identification; stars : formation; submillimeter; techniques : interferometric; techniques : spectroscopic ID MOLECULAR LINE SURVEY; ORION-KL; PROTOSTELLAR CANDIDATES; APERTURE SYNTHESIS; GHZ; MILLIMETER; OUTFLOWS; EMISSION; DUST AB Submillimeter Array (SMA) observations of the high-mass star-forming region IRAS 18089-1732 in the 1 mm and 850 mm band with 1 GHz bandwidth reveal a wealth of information. We present the observations of 34 lines from 16 different molecular species. Most molecular line maps show significant contributions from the outflow, and only a few molecules are confined to the inner core. We present and discuss the molecular line observations and outline the unique capabilities of the SMA for future imaging line surveys at high spatial resolution. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 17 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2004 VL 616 IS 1 BP L19 EP L22 DI 10.1086/422500 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800005 ER PT J AU Beuther, H Hunter, TR Zhang, Q Sridharan, TK Zhao, JH Sollins, P Ho, PTP Ohashi, N Su, YN Lim, J Liu, SY AF Beuther, H Hunter, TR Zhang, Q Sridharan, TK Zhao, JH Sollins, P Ho, PTP Ohashi, N Su, YN Lim, J Liu, SY TI Submillimeter array outflow/disk studies in the massive star-forming region IRAS 18089-1732 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; ISM : individual (IRAS 18089-1732); ISM : jets and outflows; stars : formation; submillimeter; techniques : interferometric ID PROTOSTELLAR CANDIDATES; MOLECULAR OUTFLOWS; DISK; EMISSION; CONTINUUM; SYSTEM; JET AB Submillimeter Array observations of the massive star-forming region IRAS 18089-1732 in the 1 mm and 850 mm band reveal outflow and disk signatures in different molecular lines. The SiO (5-4) data show a collimated outflow in the northern direction. In contrast, the HCOOCH3 (20-19) line, which traces high-density gas, is confined to the very center of the region and shows a velocity gradient across the core. The HCOOCH3 velocity gradient is not exactly perpendicular to the outflow axis but between an assumed disk plane and the outflow axis. We interpret these HCOOCH3 features as originating from a rotating disk that is influenced by the outflow and infall. On the basis of the (sub)millimeter continuum emission, the mass of the central core is estimated to be around 38 M,. The dynamical mass derived from the HCOOCH3 data is 22 M-circle dot, of about the same order as the core mass. Thus, the mass of the protostar/disk/envelope system is dominated by its disk and envelope. The two frequency continuum data of the core indicate a low dust opacity index beta similar to 1.2 in the outer part, decreasing to beta similar to 0.5 on shorter spatial scales. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Moran, James/0000-0002-3882-4414; Zhang, Qizhou/0000-0003-2384-6589 NR 19 TC 54 Z9 54 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 NOV 20 PY 2004 VL 616 IS 1 BP L31 EP L34 DI 10.1086/423670 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800008 ER PT J AU Beuther, H Zhang, Q Greenhill, LJ Reid, MJ Wilner, D Keto, E Marrone, D Ho, PTP Moran, JM Rao, R Shinnaga, H Liu, SY AF Beuther, H Zhang, Q Greenhill, LJ Reid, MJ Wilner, D Keto, E Marrone, D Ho, PTP Moran, JM Rao, R Shinnaga, H Liu, SY TI Subarcsecond submillimeter continuum observations of Orion KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM : individual (Orion Kleinmann-Low); stars : early-type; stars : formation; submillimeter; techniques : interferometric ID STAR-FORMATION; BN/KL REGION; HII-REGIONS; LINE SURVEY; RESOLUTION; EMISSION; IMAGES; NEBULA; OMC-1; CLOUD AB We present the first 865 mm continuum image with subarcsecond resolution obtained with the Submillimeter Array. These data resolve the Orion KL region into the hot core, the nearby radio source I, the submillimeter counterpart to the infrared source n (radio source L), and new submillimeter continuum sources. The radio to submillimeter emission from source I can be modeled as either the result of proton-electron free-free emission that is optically thick to similar to100 GHz plus dust emission that accounts for the majority of the submillimeter flux, or H- free-free emission that gives rise to a power-law spectrum with a power-law index of similar to1.6. The latter model would indicate similar physical conditions as found in the inner circumstellar environment of Mira variable stars. Future subarcsecond resolution observations at shorter submillimeter wavelengths should easily discriminate between these two possibilities. The submillimeter continuum emission toward source n can be interpreted in the framework of emission from an accretion disk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SLAC, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. 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 OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 29 TC 28 Z9 28 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 NOV 20 PY 2004 VL 616 IS 1 BP L23 EP L26 DI 10.1086/383570 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800006 ER PT J AU Gurwell, MA AF Gurwell, MA TI Submillimeter observations of Titan: Global measures of stratospheric temperature, CO, HCN, HC3N, and the isotopic ratios C-12/C-13 and N-14/N-15 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites : individual (Titan); radio lines : solar system; submillimeter techniques : interferometric ID MIXED VERTICAL PROFILE; CARBON-MONOXIDE; HETERODYNE OBSERVATIONS; ATMOSPHERE; MILLIMETER; OCCULTATION; MODELS; WINDOW AB Interferometric observations of the atmosphere of Titan were performed with the Submillimeter Array on two nights in 2004 February to investigate the global average vertical distributions of several molecular species above the tropopause. Rotational transitions of CO, isomers of HCN, and HC3N were simultaneously recorded. The abundance of CO is determined to be parts per million (ppm), constant with altitude. The vertical profile 51 +/- 4 of HCN is dependent on the assumed temperature but generally increases from 30 parts per billion at the condensation altitude (similar to83 km) to 5 ppm at similar to300 km. Furthermore, the central core of the HCN emission is strong and can be reproduced only if the upper stratospheric temperature increases with altitude. The isotopic ratios are determined to be C-12/C-13 = 132 +/- 25 and N-14/N-15 = 94 +/-13 assuming the Coustenis & Bezard temperature profile. If the Lellouch temperature profile is assumed, the ratios decrease to C-12/C-13 =108 +/- 20 and N-14/N-15 = 72 +/- 9. The vertical profile of HC3N is consistent with that derived by Marten et al. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gurwell, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mgurwell@cfa.harvard.edu NR 24 TC 54 Z9 54 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2004 VL 616 IS 1 BP L7 EP L10 DI 10.1086/423954 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800002 ER PT J AU Hirano, N Shinnaga, H Trung, DV Fong, D Keto, E Patel, N Qi, CH Young, K Zhang, QH Zhao, JH AF Hirano, N Shinnaga, H Trung, DV Fong, D Keto, E Patel, N Qi, CH Young, K Zhang, QH Zhao, JH TI High-velocity bipolar outflow and disklike envelope in the carbon star V Hydrae SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (V Hydrae); ISM : jets and outflows; ISM : molecules; stars : AGB and post-AGB ID PLANETARY-NEBULAE; EMISSION; WIND; JET; HYA AB Using the partially completed Submillimeter Array with five antennas, we have observed the CO J = 2-1 and 3-2 emission from the envelope surrounding the carbon star V Hya. The high angular resolution (2"-4") maps show that V Hya is powering a bipolar molecular jet with an extreme velocity of 70-185 km s(-1). The axis of this high-velocity jet is perpendicular to the major axis of the flattened disklike envelope, which is expanding with a velocity of similar to16 km s(-1). There is a third kinematic component, a medium-velocity wind with a deprojected velocity of 40-120 km s(-1) moving along the disk plane. Both the high-velocity jet and the medium-velocity wind have a dynamical timescale of a few hundred years. The flattened structure and the collimated jet observed in V Hya suggest that the formation of asymmetrical structure proceeds while the central star is still in the asymptotic giant branch phase. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. 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 19 TC 29 Z9 29 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 NOV 20 PY 2004 VL 616 IS 1 BP L43 EP L46 DI 10.1086/424382 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800011 ER PT J AU Ho, PTP Moran, JM Lo, KY AF Ho, PTP Moran, JM Lo, KY TI The submillimeter array SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : interferometers; submillimeter; telescopes ID RECEIVER; ANTENNAS; GHZ AB The Submillimeter Array, a collaborative project of the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, has begun operation on Mauna Kea in Hawaii. The array comprises a total of eight 6 m telescopes, which will cover the frequency range of 180-900 GHz. All eight telescopes have been deployed and are operational. First scientific results utilizing the three receiver bands at 230, 345, and 690 GHz have been obtained and are presented in the accompanying Letters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Ho, PTP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ho@cfa.harvard.edu; jmmoran@cfa.harvard.edu; flo@nrao.edu NR 39 TC 361 Z9 362 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 NOV 20 PY 2004 VL 616 IS 1 BP L1 EP L6 DI 10.1086/423245 PN 2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800001 ER PT J AU Iono, D Ho, PTP Yun, MS Matsushita, S Peck, AB Sakamoto, K AF Iono, D Ho, PTP Yun, MS Matsushita, S Peck, AB Sakamoto, K TI High-density molecular gas in the infrared-bright galaxy system VV 114 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (VV 114); galaxies : interactions; galaxies : kinematics and dynamics ID STARBURSTS; EMISSION; SAMPLE AB The new high-resolution CO (3-2) interferometric map of the IR-bright interacting galaxy system VV 114 observed with the Submillimeter Array reveals a substantial amount of warm and dense gas in the IR-bright but optically obscured galaxy, VV 114E, and the overlap region connecting the two nuclei. A 1.8 x 1.4 kpc concentration of CO (3-2) emitting gas with a total mass of 4 x 10(9) M-circle dot coincides with the peaks of near-IR, mid-IR, and radio continuum emission found previously by others, identifying the dense fuel for the active galactic nucleus and/or the starburst activity there. Extensive CO (2-1) emission is also detected, revealing detailed distribution and kinematics that are consistent with the earlier CO (1-0) results. The widely distributed molecular gas traced in CO (2-1) and the distributed discrete peaks of CO (3-2) emission suggest that a spatially extended intense starbursts may contribute significantly to its large IR luminosity. These new observations further support the notion that VV 114 is approaching its final stage of merger, when a violent central inflow of gas triggers intense starburst activity possibly boosting the IR luminosity above the ultraluminous threshold. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Iono, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 32 Z9 32 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 NOV 20 PY 2004 VL 616 IS 1 BP L63 EP L66 DI 10.1086/420784 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800016 ER PT J AU Kuan, YJ Huang, HC Charnley, SB Hirano, N Takakuwa, S Wilner, DJ Liu, SY Ohashi, N Bourke, TL Qi, CH Zhang, QH AF Kuan, YJ Huang, HC Charnley, SB Hirano, N Takakuwa, S Wilner, DJ Liu, SY Ohashi, N Bourke, TL Qi, CH Zhang, QH TI Organic molecules in low-mass protostellar hot cores: Submillimeter imaging of IRAS 16293-2422 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : abundances; ISM : individual (IRAS 16293-2422); ISM : molecules; radio lines : ISM; stars : formation ID IRAS-16293-2422; EMISSION AB Arcsecond-resolution spectral observations toward the protobinary system IRAS 16293-2422 at 344 and 354 GHz were conducted using the Submillimeter Array. Several complex organic molecules, such as CH3OH and HCOOCH3, were detected and mapped. Together with the rich organic inventory revealed, it clearly indicates the existence of two, rather than one, compact hot molecular cores (less than or similar to400 AU in radius) associated with each of the protobinary components identified by their dust continuum emission in the inner star-forming core. C1 Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kuan, YJ (reprint author), Natl Taiwan Normal Univ, Dept Earth Sci, 88 Sect 4,Ting Chou Rd, Taipei 116, Taiwan. EM kuan@sgrb2.geos.ntnu.edu.tw; hspring@sgrb2.geos.ntnu.edu.tw; charnley@dusty.arc.nasa.gov; hirano@asiaa.sinica.edu.tw; stakakuw@sma.hawaii.edu; dwilner@cfa.harvard.edu; syliu@asiaa.sinica.edu.tw; ohashi@asiaa.sinica.edu.tw; tbourke@cfa.harvard.edu; cqi@cfa.harvard.edu; qzhang@cfa.harvard.edu RI Charnley, Steven/C-9538-2012; OI Zhang, Qizhou/0000-0003-2384-6589 NR 11 TC 77 Z9 77 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 NOV 20 PY 2004 VL 616 IS 1 BP L27 EP L30 DI 10.1086/426315 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800007 ER PT J AU Matsushita, S Sakamoto, K Kuo, CY Hsieh, PY Trung, DV Mao, RQ Iono, D Peck, AB Wiedner, MC Liu, SY Ohashi, N Lim, J AF Matsushita, S Sakamoto, K Kuo, CY Hsieh, PY Trung, DV Mao, RQ Iono, D Peck, AB Wiedner, MC Liu, SY Ohashi, N Lim, J TI Submillimeter array (CO)-C-12 (J=3-2) interferometric observations of the central region of M51 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M51, NGC 5194); galaxies : ISM; galaxies : nuclei; galaxies : Seyfert; ISM : jets and outflows ID DENSE MOLECULAR GAS; NEARBY GALAXIES; SPIRAL GALAXIES; ACTIVE NUCLEUS; STAR-FORMATION; CO; EMISSION; NGC-1068; KINEMATICS; EXCITATION AB We present the first interferometric (CO)-C-12 (J = 3-2) observations (beam size of 3."9 x 1."6 or 160 x 65 pc) with the Submillimeter Array (SMA) toward the center of the Seyfert 2 galaxy M51. The image shows a strong concentration at the nucleus and weak emission from the spiral arm to the northwest. The integrated intensity of the central component in (CO)-C-12 (J = 3-2) is almost twice as high as that in (CO)-C-12 (J = 1-0), indicating that the molecular gas within an similar to80 pc radius of the nucleus is warm (greater than or similar to100 K) and dense (similar to10(4) cm(-3)). Similar intensity ratios are seen in shocked regions in our Galaxy, suggesting that these gas properties may be related to active galactic nucleus or starburst activity. The central component shows a linear velocity gradient (similar to1.4 km s(-1) pc(-1)) perpendicular to the radio continuum jet, similar to that seen in previous observations and interpreted as a circumnuclear molecular disk/torus around the Seyfert 2 nucleus. In addition, we identify a linear velocity gradient (0.7 km s(-1) pc(-1)) along the jet. Judging from the energetics, the velocity gradient can be explained by supernova explosions or energy and momentum transfer from the jet to the molecular gas via interaction, which is consistent with the high-intensity ratio. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Taiwan Normal Univ, Dept Phys, Taipei 116, Taiwan. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Univ Cologne, Inst Phys, D-50937 Cologne, Germany. RP Matsushita, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM satoki@asiaa.sinica.edu.tw NR 35 TC 28 Z9 28 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 NOV 20 PY 2004 VL 616 IS 1 BP L55 EP L58 DI 10.1086/424798 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800014 ER PT J AU Qi, CH Ho, PTP Wilner, DJ Takakuwa, S Hirano, N Ohashi, N Bourke, TL Zhang, QH Blake, GA Hogerheijde, M Saito, M Choi, MH Yang, J AF Qi, CH Ho, PTP Wilner, DJ Takakuwa, S Hirano, N Ohashi, N Bourke, TL Zhang, QH Blake, GA Hogerheijde, M Saito, M Choi, MH Yang, J TI Imaging the disk around 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 MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; RADIATIVE-TRANSFER; YOUNG STARS; X-RAY; TAURI; EMISSION; CALIBRATION; MODELS AB We present similar to2"-4" aperture synthesis observations of the circumstellar disk surrounding the nearby young star TW Hya in the CO J = 2-1 and J = 3-2 lines and associated dust continuum obtained with the partially completed Submillimeter Array. The extent and peak flux of the 230 and 345 GHz dust emission follow closely the predictions of the irradiated accretion disk model of Calvet et al. The resolved molecular line emission extends to a radius of at least 200 AU, the full extent of the disk visible in scattered light, and shows a clear pattern of Keplerian rotation. Comparison of the images with two-dimensional Monte Carlo models constrains the disk inclination angle to 7degrees +/- 1degrees. The CO emission is optically thick in both lines, and the kinetic temperature in the line formation region is similar to20 K. Substantial CO depletion, by an order of magnitude or more from canonical dark cloud values, is required to explain the characteristics of the line emission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Sunmillimeter Array Project, Hilo, HI 96720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. 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. Natl Astron Observ Japan, Tokyo 1818588, Japan. Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea. Chinese Acad Sci, Purple Mt Observ, Nanjing 21008, Peoples R China. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM cqi@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 21 TC 123 Z9 123 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 NOV 20 PY 2004 VL 616 IS 1 BP L11 EP L14 DI 10.1086/421063 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800003 ER PT J AU Sakamoto, K Matsushita, S Peck, AB Wiedner, MC Iono, D AF Sakamoto, K Matsushita, S Peck, AB Wiedner, MC Iono, D TI Molecular gas around the double nucleus in M83 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M83, NGC 5236); galaxies : ISM; galaxies : kinematics and dynamics; galaxies : nuclei; galaxies : starburst ID SPIRAL GALAXIES; STARBURST; KINEMATICS; EMISSION; M-83; DISK; CO; REMNANTS; MERGERS; BAR AB The center of M83, a barred starburst galaxy with a double nucleus, has been observed in the CO (J = 2-1) and CO (J = 3-2) lines with the Submillimeter Array. The molecular gas shows a distribution and kinematics typical for barred galaxies at similar to1 kpc radii but reveals unusual kinematics around the double nucleus in the central similar to300 pc. Our CO velocity data show that the visible nucleus in M83 is at least 3" (65 pc) away from the galaxy's dynamical center, which most likely coincides with the center of symmetry previously determined in the K band and is suggested to host another nucleus. We discovered high-velocity molecular gas associated with the visible off-center nucleus and also found a steep velocity gradient across it. We attribute these features to a gas disk rotating around the off-center nucleus, which may be the remnant of a small galaxy accreted by M83. The dynamical mass of this component is estimated to be 2 x 10(8) M-circle dot within a radius of 40 pc. The dynamical perturbation from the off-center nucleus may have played a key role in shaping the lopsided starburst. C1 Harvard Smithsonian Ctr Astrophys, Submilleter Array, Hilo, HI 96720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Cologne, Inst Phys, D-50937 Cologne, Germany. Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. RP Sakamoto, K (reprint author), Harvard Smithsonian Ctr Astrophys, Submilleter Array, 645 N Aohoku Pl, Hilo, HI 96720 USA. NR 27 TC 33 Z9 33 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 NOV 20 PY 2004 VL 616 IS 1 BP L59 EP L62 DI 10.1086/420845 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800015 ER PT J AU Shinnaga, H Moran, JM Young, KH Ho, PTP AF Shinnaga, H Moran, JM Young, KH Ho, PTP TI Interferometric observation of the highly polarized SiO maser emission from the nu=1, J=5-4 transition associated with VY Canis Majoris SO ASTROPHYSICAL JOURNAL LA English DT Article DE masers; polarization; radio lines : general; stars : individual (VY Canis Majoris); stars : late-type; techniques : interferometric ID LATE-TYPE STARS; SUBMILLIMETER OBSERVATIONS; ASTROPHYSICAL MASERS; ASTRONOMICAL MASERS; LINEAR-POLARIZATION; CIRCUMSTELLAR DUST; MAGNETIC-FIELD; EVOLVED STARS; SUPERGIANTS; J=1-0 AB We used the Submillimeter Array to image the SiO maser emission in the v = 1 J = 5-4, transition associated with the peculiar red supergiant VY Canis Majoris. We identified seven maser components and measured their relative positions and linear polarization properties. Five of the maser components are coincident to within about 150 mas (similar to200 AU at the distance of 1.5 kpc); most of them may originate in the circumstellar envelope at a radius of about 50 mas from the star along with the SiO masers in the lowest rotational transitions. Our measurements show that two of the maser components may be offset from the inner stellar envelope (at the 3 sigma level of significance) and may be part of a larger bipolar outflow associated with VY CMa identified by Shinnaga et al. The strongest maser feature at a velocity of 35.9 km s(-1) has a 60% linear polarization, and its polarization direction is aligned with the bipolar axis. Such a high degree of polarization suggests that maser inversion is due to radiative pumping. Five of the other maser features have significant linear polarization. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96720 USA. RP Shinnaga, H (reprint author), CALTECH, Submillimeter Observ, 111 Nowelo St, Hilo, HI 96720 USA. EM hshinnaga@cfa.harvard.edu NR 33 TC 15 Z9 15 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 NOV 20 PY 2004 VL 616 IS 1 BP L47 EP L50 DI 10.1086/425133 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800012 ER PT J AU Sollins, PK Hunter, TR Battat, J Beuther, H Ho, PTP Lim, J Liu, SY Ohashi, N Sridharan, TK Su, YN Zhao, JH Zhang, Q AF Sollins, PK Hunter, TR Battat, J Beuther, H Ho, PTP Lim, J Liu, SY Ohashi, N Sridharan, TK Su, YN Zhao, JH Zhang, Q TI Mapping the outflow from G5.89-0.39 in SiO J=5 -> 4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM : individual (G5.89-0.39); ISM : jets and outflows; stars : formation ID H-II REGIONS; STAR-FORMATION REGIONS; YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; MASSIVE STARS; VELOCITY; EVOLUTION; DISTANCE; SAMPLE AB We have mapped the ultracompact H II region, G5.89-0.39, and its molecular surroundings with the Submillimeter Array at 2."8 x 1."8 angular resolution in 1.3 mm continuum, SiO J = 5 --> 4, and eight other molecular lines. We have resolved for the first time the highly energetic molecular outflow in this region. At this resolution, the outflow is definitely bipolar and appears to originate in a 1.3 mm continuum source. The continuum source peaks in the center of the H II region. The axis of the outflow lines up with a recently discovered O5 V star. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. ASIAA, Hilo, HI 96720 USA. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM psollins@cfa.harvard.edu NR 32 TC 28 Z9 28 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 NOV 20 PY 2004 VL 616 IS 1 BP L35 EP L38 DI 10.1086/421294 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800009 ER PT J AU Su, YN Liu, SY Lim, J Ohashi, N Beuther, H Zhang, Q Sollins, P Hunter, T Sridharan, TK Zhao, JH Ho, PTP AF Su, YN Liu, SY Lim, J Ohashi, N Beuther, H Zhang, Q Sollins, P Hunter, T Sridharan, TK Zhao, JH Ho, PTP TI Search for calibrators for the submillimeter array. I. High-mass star-forming regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; radio continuum : ISM; techniques : interferometric ID ULTRACOMPACT HII-REGIONS; PROTOSTELLAR CANDIDATES; DUST CONTINUUM; FLUX DENSITIES; MASERS; RECOMBINATION; MILLIMETERS; RESOLUTION; EVOLUTION; IMAGES AB We present initial results of an ongoing search for interferometric calibrators at submillimeter wavelengths with the Submillimeter Array (SMA). Powerful radio galaxies are commonly used as calibrators at centimeter and millimeter wavelengths, but many are not strong enough to serve as calibrators at submillimeter wavelengths because of their rapidly declining flux densities toward shorter wavelengths. The inability to find a calibrator close to the target source may limit or even prevent us from imaging many interesting sources at submillimeter wavelengths. Here, we investigate whether high-mass protostellar objects and ultracompact H II regions can serve as useful calibrators for the SMA. The dust emission associated with these objects makes them among the brightest submillimeter sources in the sky. Our observations at 0.85 mm (345 GHz) with an angular resolution of similar to3" reveal that although a large fraction of the dust emission originates from an extended "halo" component, a compact unresolved component often remains that when sufficiently strong may serve as a useful calibrator. These observations also provide a first glimpse at the small-scale distribution of dust around ultracompact H II regions and high-mass protostellar objects at submillimeter wavelengths. We discuss the origin of the core-halo structure seen in many sources and conclude with suggestions for future searches for calibrators with the SMA. C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Natl Cent Univ, Inst Astron, Taoyuan 320, Taiwan. Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 NR 32 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2004 VL 616 IS 1 BP L39 EP L42 DI 10.1086/422030 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800010 ER PT J AU Takakuwa, S Ohashi, N Ho, PTP Qi, CH Wilner, DJ Zhang, QH Bourke, TL Hirano, N Choi, M Yang, J AF Takakuwa, S Ohashi, N Ho, PTP Qi, CH Wilner, DJ Zhang, QH Bourke, TL Hirano, N Choi, M Yang, J TI Submillimeter array observations of L1551 IRS 5 in CS J=7-6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (L1551 IRS 5); ISM : molecules; planetary systems : protoplanetary disks; stars : formation ID YOUNG STELLAR OBJECTS; DISK-LIKE ENVELOPE; DETAILED STRUCTURE; BINARY-SYSTEM; GAS DISK; L1551-IRS-5; CO; PROTOSTAR; OUTFLOW; SHOCKS AB We have imaged the circumstellar envelope around the binary protostar L1551 IRS 5 in CS J = 7-6 and 343 GHz continuum emission at similar to3" resolution using the Submillimeter Array. The continuum emission shows an elongated structure (similar to22- x 100 AU) around the binary perpendicular to the axis of the associated radio jet. The CS emission extends over similar to400 AU, appears approximately circularly symmetric, and shows a velocity gradient from southeast (blueshifted) to northwest (redshifted). The direction of the velocity gradient is different from that observed in (CO)-O-18 J = 1-0. This may be because rotation is more dominant in the CS envelope than the (CO)-O-18 envelope, in which both infall and rotation exist. The CS emission can be divided into two velocity components: (1) a "high"- velocity disklike structure surrounding the protostar +/- 1.0-1.5 km s(-1) from the systemic velocity, and (2) a "low"-velocity structure located southwest of the protostar less than 1.0 km s(-1) from the systemic velocity. The high-velocity component traces warm and dense gas with kinematics consistent with rotation around the protostar. The low-velocity component may arise from dense gas entrained in the outflow. Alternatively, this component may trace infalling and rotating gas in an envelope with a vertical structure. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, Hilo, HI 96720 USA. Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea. Chinese Acad Sci, Purple Mt Observ, Nanjing 21008, Peoples R China. RP Takakuwa, S (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array Project, 645 N Aohoku, Hilo, HI 96720 USA. EM stakakuwa@sma.hawaii.edu; nohashi@sma.hawaii.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 30 TC 26 Z9 26 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 NOV 20 PY 2004 VL 616 IS 1 BP L15 EP L18 DI 10.1086/421939 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800004 ER PT J AU Wang, JZ Zhang, QH Wang, Z Ho, PTP Fazio, GG Wu, YF AF Wang, JZ Zhang, QH Wang, Z Ho, PTP Fazio, GG Wu, YF TI Warm molecular gas in galaxy-galaxy merger NGC 6090 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 6090); galaxies : interactions; galaxies : kinematics and dynamics ID LUMINOUS INFRARED GALAXIES; ANTENNAE GALAXIES; STAR-FORMATION; CO AB We present Submillimeter Array observations of the CO (2-1) and (3-2) transitions toward the merging galaxies of NGC 6090. The high-resolution CO data reveal three gas concentrations. The main component is peaking in the overlap region between the two galaxies, where the near-IR and radio continuum emission are weak. The CO (2-1) emission from the face-on galaxy NGC 6090E is somewhat stronger than that from the edge-on galaxy NGC 6090W. The CO (3-2) emission peaks in the overlap region, similar to the CO (2-1) emission. More than 50% of the CO (3-2) emission arises from the 2" (1.2 kpc) area of the overlap region. There appears to be CO (3-2) emission toward the nuclear region and the northwest arm of NGC 6090E, while no CO (3-2) emission is detected toward NGC 6090W. Unlike the CO gas, most of the radio continuum emission comes from NGC 6090E. The strong CO emission, together with the weak radio continuum emission, suggests that star formation in the overlap region has not proceeded long enough to produce significant numbers of supernovae that would be detectable from their radio continuum emission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Peking Univ, Dept Astron, Beijing 100871, Peoples R China. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Wang, JZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jwang@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 17 TC 10 Z9 10 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 NOV 20 PY 2004 VL 616 IS 1 BP L67 EP L70 DI 10.1086/422681 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800017 ER PT J AU Young, KH Hunter, TR Wilner, DJ Gurwell, MA Barrett, JW Blundell, R Christensen, R Fong, D Hirano, N Ho, PTP Liu, SY Lo, KY Martin, R Matsushita, S Moran, JM Ohashi, N Papa, DC Patel, N Patt, F Peck, A Qi, C Saito, M Schinckel, A Shinnaga, H Sridharan, TK Takakuwa, S Tong, CE Trung, DV AF Young, KH Hunter, TR Wilner, DJ Gurwell, MA Barrett, JW Blundell, R Christensen, R Fong, D Hirano, N Ho, PTP Liu, SY Lo, KY Martin, R Matsushita, S Moran, JM Ohashi, N Papa, DC Patel, N Patt, F Peck, A Qi, C Saito, M Schinckel, A Shinnaga, H Sridharan, TK Takakuwa, S Tong, CE Trung, DV TI Submillimeter array observations of CS J=14-13 emission from the evolved star IRC+10216 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; stars : individual (IRC+10216); techniques : interferometric ID VIBRATIONALLY EXCITED CS; SPECTRAL-LINE SURVEY; CIRCUMSTELLAR ENVELOPE; MILLIMETER; IRC; WAVELENGTHS; SHELLS; GHZ AB We present imaging observations of the evolved star IRC +10216 in the CS J = 14-13 line at 685.4 GHz and the associated submillimeter continuum at similar to2" resolution made with the partially constructed Submillimeter Array. The CS J = 14-13 line emission from the stellar envelope is well resolved both spatially and spectrally. The strong central concentration of the line emission provides direct evidence that CS is a parent molecule that forms close to the stellar photosphere, in accord with previous images of the lower excitation CS J = 2-1 line and inferences from unresolved observations of vibrationally excited transitions. The continuum emission is dominated by a compact, unresolved component, consistent with the photospheric emission, that accounts for similar to20% of the broadband 450 mum flux. These are the first interferometer imaging observations made in the semitransparent 450 mum atmospheric window. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Natl Astron Observ Japan, Tokyo 1818588, Japan. RP Young, KH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dwilner@cfa.harvard.edu OI Tong, Edward/0000-0002-7736-4203; Hunter, Todd/0000-0001-6492-0090; Moran, James/0000-0002-3882-4414 NR 22 TC 9 Z9 9 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 NOV 20 PY 2004 VL 616 IS 1 BP L51 EP L54 DI 10.1086/420883 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 872IB UT WOS:000225199800013 ER PT J AU Kiessling, W Baron-Szabo, RC AF Kiessling, W Baron-Szabo, RC TI Extinction and recovery patterns of scleractinian corals at the Cretaceous-Tertiary boundary SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article; Proceedings Paper CT Workshop on Mesozoic-Cenozoic Bioevents CY 2002 CL Berlin, GERMANY DE Cretaceous-Tertiary boundary; mass extinction; corals; evolution; reefs ID MARINE BIVALVE EXTINCTIONS; MASS EXTINCTIONS; REEF; ORIGINATION; DIVERSITY; EVOLUTION; HISTORY; SPAIN; BASIN; SEDIMENTOLOGY AB The extinction and recovery of scleractinian corals at the Cretaceous-Tertiary (K-T) boundary was analyzed based on a Global database of taxonomically revised late Campanian to Paleocene coral collections. In contrast to earlier statements, our results indicate that extinction rates of corals were only moderate in comparison to other marine invertebrates. We have calculated a 30% extinction rate for Maastrichtian coral genera occurring in more than one stratigraphic stage and more than one geographic region. Reverse rarefaction suggests that some 45% of all coral species became extinct. Photosymbiotic (zooxanthellate) corals were significantly more affected by the extinction than azooxanthellate corals; colonial forms were hit harder than solitary forms, and among colonial forms an elevated integration of corallites raised extinction risk. Abundance, as measured by the number of taxonomic occurrences, had apparently no influence on survivorship, but a wide geographic distribution significantly reduced extinction risk. As in bivalves and echinoids neither species richness within genera nor larval type had an effect on survivorship. An indistinct latitudinal gradient is visible in the extinction, but this is exclusively due to a higher proportion of extinction-resistant azooxanthellate corals in higher-latitude assemblages. No significant geographic hotspot could be recognized, neither in overall extinction rates nor in the extinction of endemic clades. More clades than previously recognized passed through the K-T boundary only to become extinct within the Danian. These failed survivors were apparently limited to regions outside the Americas. Recovery as defined by the proportional increase of newly evolved genera, was more rapid for zooxanthellate corals than previously assumed and less uniform geographically than the extinction. Although newly evolved Danian azooxanthellate genera were significantly more common than new zooxanthellate genera, the difference nearly disappeared by the late Paleocene suggesting a more rapid recovery of zooxanthellate corals in comparison to previous analyses. New Paleocene genera were apparently concentrated in low latitudes, suggesting that the tropics formed a source of evolutionary novelty in the recovery phase. (C) 2004 Elsevier B.V. All rights reserved. C1 Humboldt Univ, Museum Hist Nat, Inst Paleontol, D-10115 Berlin, Germany. Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Washington, DC 20560 USA. RP Kiessling, W (reprint author), Humboldt Univ, Museum Hist Nat, Inst Paleontol, Invalidenstr 43, D-10115 Berlin, Germany. EM wolfgang.kiessling@museum.hu-berlin.de RI Kiessling, Wolfgang/E-2259-2015 NR 155 TC 56 Z9 58 U1 2 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD NOV 18 PY 2004 VL 214 IS 3 BP 195 EP 223 DI 10.1016/j.palaeo.2004.05.025 PG 29 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 872II UT WOS:000225200500003 ER PT J AU Holcomb, M Pandolfi, JM Macintyre, IG Budd, AF AF Holcomb, M Pandolfi, JM Macintyre, IG Budd, AF TI Use of X-radiographs to distinguish members of the Montastraea annularis reef-coral species complex SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 7th International Conference on Coelenterate Biology CY JUL 06-11, 2003 CL Univ Kansas, Lawrence, KS HO Univ Kansas DE Montastraea; coral reef; Pleistocene; coral banding; species complex ID BUILDING CORAL; GROWTH-RATES; SCLERACTINIA; COLONIES; JAMAICA; CLIMATE; FORM; BAY AB Recent work suggests the Montastraea annularis species complex consists of at least three species, which can be distinguished qualitatively in the field using features related to colony growth (e.g. overall growth form. bumpiness, growth along the colony edge). However, when whole colonies are not available and surfaces are eroded, identification becomes problematic when relying on such characteristics. Characters based on internal skeletal structures are less prone to loss due to taphonomic processes. Previous work has shown that internal corallite architectural features measured in transverse thin sections can be used to distinguish species. To determine whether internal colony-level features measured on X-radiographs can be used. eight characters related to corallite budding and accretionary growth were measured on specimens representing three modern members of the M. annularis species complex (M. annularis, M. flaveolata and M. franksi), as well as two fossil forms (columnar and organ-pipe). All eight characters showed significant differences among species. Discriminant function analysis using seven of these characters resulted in distinct species groupings In canonical scores plots and a 100% classification success for specimens from Panama. These results suggest that measurements made on X-radiographs provide a useful tool for quantitatively distinguishing members of the M. annularis complex as well as between other massive reef corals. C1 Univ Queensland, Ctr Marine Sci, Brisbane, Qld 4072, Australia. Univ Queensland, Dept Earth Sci, Brisbane, Qld 4072, Australia. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. RP Pandolfi, JM (reprint author), Univ Queensland, Ctr Marine Sci, Brisbane, Qld 4072, Australia. EM j.pandolfi@marine.uq.edu.au RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 27 TC 5 Z9 7 U1 0 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD NOV 15 PY 2004 VL 530 SI SI BP 211 EP 222 DI 10.1007/s10750-004-2652-x PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 889AU UT WOS:000226416700026 ER PT J AU Sanchez, JA AF Sanchez, JA TI Evolution and dynamics of branching colonial form in marine modular cnidarians: gorgonian octocorals SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 7th International Conference on Coelenterate Biology CY JUL 06-11, 2003 CL Univ Kansas, Lawrence, KS HO Univ Kansas DE colonial organisms; heterochrony; Cnidaria ID RIBOSOMAL-RNA; PHENOTYPIC INTEGRATION; PHYLOGENETIC ANALYSES; REDOX CONTROL; HOX GENE; ORGANISMS; GROWTH; ORGANIZATION; HYDROIDS; ANTHOZOA AB Multi-branched arborescent networks are common patterns for many sessile marine modular organisms but no clear understanding of their development is yet available. This paper reviews new findings in the theoretical and comparative biology of branching modular organisms (e.g. Octocorallia: Cnidaria) and new hypotheses on the evolution of form are discussed. A particular characteristic of branching Caribbean gorgonian octocorals is a morphologic integration at two levels of colonial organization based on whether the traits are at the module or colony level. This revealed an emergent level of integration and modularity produced by the branching process itself and not entirely by the module replication. In essence, not just a few changes at the module level could generate changes in colony architecture. suggesting uncoupled developmental patterning for the polyp and branch level traits. Therefore. the evolution of colony form in octocorals seems to be related to the changes affecting the process of branching. Branching in these organisms is sub-apical, coming from mother branches, and the highly self-organized form is the product of a dynamic process maintaining a constant ratio between mother and daughter branches. Colony growth preserves shape but is a logistic growth-like event due to branch interference and/or allometry. The qualitative branching patterns in octocorals (e.g. sea feathers, fans, sausages, and candelabra) occurred multiple times when compared with recent molecular phylogenies, suggesting independence of common ancestry to achieve these forms. A number of species with different colony forms. particularly alternate species (e.g. sea candelabrum), shared the same value for an important branching parameter (the ratio of mother to total branches). According to the way gorgonians branch and achieve form, it is hypothesized that the diversity of alternate species sharing the same narrow variance in that critical parameter for growth might be the product of canalization (or a developmental constraint), where uniform change in growth rates and maximum colony size might explain colony differences among species. If the parameter presenting shape in the colonies is fixed but colonies differ in their growth rates and maximum sizes. heterochrony could be responsible for the evolution among some gorgonian corals with alternate branching. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC 163, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, MRC 163, Washington, DC 20560 USA. RP Sanchez, JA (reprint author), Univ Los Andes, Dept Ciencias Biol, Carrera 1E 18A-10,POB 4876, Bogota, Colombia. EM juansanc@uniandes.edu.co NR 48 TC 21 Z9 21 U1 5 U2 16 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD NOV 15 PY 2004 VL 530 SI SI BP 283 EP 290 DI 10.1007/s10750-004-2684-2 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 889AU UT WOS:000226416700034 ER PT J AU Jaegle, L Martin, RV Chance, K Steinberger, L Kurosu, TP Jacob, DJ Modi, AI Yoboue, V Sigha-Nkamdjou, L Galy-Lacaux, C AF Jaegle, L Martin, RV Chance, K Steinberger, L Kurosu, TP Jacob, DJ Modi, AI Yoboue, V Sigha-Nkamdjou, L Galy-Lacaux, C TI Satellite mapping of rain-induced nitric oxide emissions from soils SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE soil; NOx; satellite ID TROPICAL TROPOSPHERIC OZONE; BIOMASS-BURNING EMISSIONS; TRACE-GAS EMISSIONS; NITROGEN MONOXIDE; GLOBAL INVENTORY; SOUTH ATLANTIC; SAVANNA SOILS; N2O EMISSIONS; WEST-AFRICA; MODEL AB [1] We use space-based observations of NO2 columns from the Global Ozone Monitoring Experiment (GOME) to map the spatial and seasonal variations of NOx emissions over Africa during 2000. The GOME observations show not only enhanced tropospheric NO2 columns from biomass burning during the dry season but also comparable enhancements from soil emissions during the rainy season over the Sahel. These soil emissions occur in strong pulses lasting 1 - 3 weeks following the onset of rain, and affect 3 million km(2) of semiarid sub-Saharan savanna. Surface observations of NO2 from the International Global Atmospheric Chemistry (IGAC)/Deposition of Biochemically Important Trace Species (DEBITS)/Africa (IDAF) network over West Africa provide further evidence for a strong role for microbial soil sources. By combining inverse modeling of GOME NO2 columns with space-based observations of fires, we estimate that soils contribute 3.3 +/- 1.8 TgN/year, similar to the biomass burning source (3.8 +/- 2.1 TgN/year), and thus account for 40% of surface NOx emissions over Africa. Extrapolating to all the tropics, we estimate a 7.3 TgN/year biogenic soil source, which is a factor of 2 larger compared to model-based inventories but agrees with observation-based inventories. These large soil NOx emissions are likely to significantly contribute to the ozone enhancement originating from tropical Africa. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Univ Abdou Moumouny Niamey, Ecole Normale Super, Dept Phys, Niamey, Niger. Univ Cocody, Lab Phys Atmosphere, Abidjan, Cote Ivoire. Ctr Rech Hydrol, Yaounde, Cameroon. Univ Toulouse 3, Observ Midi Pyrenees, Lab Aerol, CNRS,UMR 5560, F-31400 Toulouse, France. RP Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM jaegle@atmos.washington.edu; rvmartin@fizz.phys.dal.ca; kchance@cfa.harvard.edu; llou@atmos.washington.edu; tkurosu@cfa.harvard.edu; djacob@fas.harvard.edu; aimod@yahoo.com; yobouev@hotmail.com; lucsigha@hotmail.com; llacc@aero.obs-mip.fr RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Chance, Kelly/0000-0002-7339-7577 NR 63 TC 81 Z9 85 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 12 PY 2004 VL 109 IS D21 AR D21310 DI 10.1029/2004JD004787 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 872EM UT WOS:000225190500005 ER PT J AU Sozzetti, A AF Sozzetti, A TI On the possible correlation between the orbital periods of extrasolar planets and the metallicity of the host stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : statistical; stars : abundances; planetary systems : formation ID SPACE-INTERFEROMETRY-MISSION; NARROW-ANGLE ASTROMETRY; STELLAR METALLICITY; STATISTICAL PROPERTIES; GIANT PLANETS; ABUNDANCE ANALYSES; SOLAR PLANETS; PARENT STARS; SYSTEMS; MASS AB We investigate a possible correlation between the orbital periods P of the extrasolar planet sample and the metallicity [Fe/H] of their parent stars. Close-in planets, on orbits of a few days, are more likely to be found around metal-rich stars. Simulations show that a weak correlation is present. This correlation becomes stronger when only single stars with one detected planet are considered. We discuss several potential sources of bias that might mimic the correlation, and find that they can be ruled out, but not with high significance. If real, the absence of very short-period planets around the stellar sample with [Fe/H] < 0.0 can be interpreted as evidence of a metallicity dependence of the migration rates of giant planets during formation in the protoplanetary disc. The observed P-[Fe/H] correlation can be falsified or confirmed by conducting spectroscopic or astrometric surveys of metal-poor stars ([Fe/H] < -0.5) in the field. C1 Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. RP Sozzetti, A (reprint author), Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. EM alex@phyast.pitt.edu OI Sozzetti, Alessandro/0000-0002-7504-365X NR 52 TC 35 Z9 35 U1 1 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2004 VL 354 IS 4 BP 1194 EP 1200 DI 10.1111/j.1365-2966.2004.08281.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 868OJ UT WOS:000224922600026 ER PT J AU Argon, AL Greenhill, LJ Moran, JM Reid, MJ Menten, KM Inoue, M AF Argon, AL Greenhill, LJ Moran, JM Reid, MJ Menten, KM Inoue, M TI The IC 133 water vapor maser in the galaxy M33: A geometric distance SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M33); ISM : individual (IC 133); masers ID PERIOD-LUMINOSITY RELATIONS; LARGE-MAGELLANIC-CLOUD; RED GIANT BRANCH; PROPER MOTIONS; EXTERNAL GALAXIES; CEPHEID DISTANCE; H2O; SCALE; W49N; KINEMATICS AB We report on the results of a 14 yr long VLBI study of proper motions in the IC 133 H2O maser source in the galaxy M33. The method of ordered motion parallax was used to model the three-dimensional structure and dynamics of IC 133 and to obtain a distance estimate, 800 +/- 180 kpc. Our technique for determining the distance to M33 is independent of calibrations common to other distance indicators, such as Cepheid period-luminosity relations, and therefore provides an important check for previous distance determinations. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Natl Astron Observ, Nobeyama Radio Observ, Minamisa Ku, Nagano 38413, Japan. RP Argon, AL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 39 TC 11 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 NOV 10 PY 2004 VL 615 IS 2 BP 702 EP 719 DI 10.1086/424731 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300013 ER PT J AU Williams, BF Sjouwerman, LO Kong, AKH Gelfand, JD Garcia, MR Murray, SS AF Williams, BF Sjouwerman, LO Kong, AKH Gelfand, JD Garcia, MR Murray, SS TI Two new X-ray/optical/radio supernova remnants in M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M31); supernova remnants; techniques : image processing ID INTERSTELLAR-MEDIUM; RAY SOURCES; CANDIDATES; DISCOVERY; EMISSION; CHANDRA; REGION AB We compare a deep ( 37 ks) Chandra ACIS-S image of the M31 bulge to Local Group Survey narrowband optical data and Very Large Array (VLA) radio data of the same region. Our precisely registered images reveal two new optical shells with X-ray counterparts. These shells have sizes, [S II]/Halpha flux ratios, and X-ray spectral properties typical of supernova remnants (SNRs) with ages of 9(-4)(+3) and 17(-9)(+6) kyr. Analysis of complementary VLA data reveals the radio counterparts, further confirming that they are SNRs. We discuss and compare the properties and morphologies of these SNRs at the different wavelengths. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Williams, BF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM williams@head.cfa.harvard.edu; lsjouwer@aoc.nrao.edu; akong@head.cfa.harvard.edu; jgelfand@cfa.harvard.edu; garcia@head.cfa.harvard.edu; ssm@head.cfa.harvard.edu RI Gelfand, Joseph/F-1110-2015 OI Gelfand, Joseph/0000-0003-4679-1058 NR 26 TC 8 Z9 8 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 NOV 10 PY 2004 VL 615 IS 2 BP 720 EP 726 DI 10.1086/424589 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300014 ER PT J AU Chu, YH Gruendl, RA Chen, CHR Lazendic, JS Dickel, JR AF Chu, YH Gruendl, RA Chen, CHR Lazendic, JS Dickel, JR TI An optical and X-ray examination of two radio supernova remnant candidates in 30 Doradus SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; HII regions; ISM : individual (30 Doradus); Magellanic Clouds; supernova remnants ID LARGE-MAGELLANIC-CLOUD; PLANETARY CAMERA 2; H-II-REGION; STAR-FORMATION; 30-DORADUS NEBULA; NOVA REMNANTS; HOT PLASMA; IMAGES; MASS; EXTINCTION AB The giant H II region 30 Doradus is known for its violent internal motions and bright diffuse X-ray emission, suggesting the existence of supernova remnants (SNRs), but no nonthermal radio emission has been detected. Recently, Lazendic et al. compared the Halpha/Hbeta and radio/Halpha ratios and suggested two small radio sources to be nonthermal and thus SNR candidates; however, no optical or X-ray counterparts were detected. We have used high-resolution optical images and high-dispersion spectra to examine the morphological, spectral, and kinematic properties of these two SNR candidates and still find no optical evidence supporting their identification as SNRs. We have also determined the X-ray luminosities of these SNR candidates and find them 1 - 3 orders of magnitude lower than those commonly seen in young SNRs. High extinction can obscure optical and X-ray signatures of an SNR, but would prohibit the use of a high radio/Halpha ratio to identify nonthermal radio emission. We suggest that the SNR candidate MCRX J053831.8 - 690620 is associated with a young star-forming region; while the radio emission originates from the obscured star-forming region, the observed optical emission is dominated by the foreground. We suggest that the SNR candidate MCRX J053838.8 - 690730 is associated with a dust/molecular cloud, which obscures some optical emission but not the radio emission. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chu, YH (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM chu@astro.uiuc.edu; gruendl@astro.uiuc.edu; c-chen@astro.uiuc.edu; jlazendic@cfa.harvard.edu; johnd@astro.uiuc.edu NR 36 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2004 VL 615 IS 2 BP 727 EP 731 DI 10.1086/424654 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300015 ER PT J AU Fatuzzo, M Adams, FC Myers, PC AF Fatuzzo, M Adams, FC Myers, PC TI Generalized collapse solutions with nonzero initial velocities for star formation in molecular cloud cores SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; stars : formation ID SINGULAR ISOTHERMAL TOROIDS; MAGNETIC INTERSTELLAR CLOUDS; GRAVITATING GASEOUS SPHERES; SELF-SIMILAR COLLAPSE; EQUATION-OF-STATE; DENSE CORES; AMBIPOLAR DIFFUSION; INFALL MOTIONS; DARK CLOUDS; PROTO-STAR AB Motivated by recent observations that show that starless molecular cloud cores exhibit subsonic inward velocities, we revisit the collapse problem for polytropic gaseous spheres. In particular, we provide a generalized treatment of protostellar collapse in the spherical limit and find semianalytic (self-similar) solutions, corresponding numerical solutions, and purely analytic calculations of the mass infall rates ( the three approaches are in good agreement). This study focuses on collapse solutions that exhibit nonzero inward velocities at large radii, as observed in molecular cloud cores, and extends previous work in four ways: ( 1) the initial conditions allow nonzero initial inward velocity, ( 2) the starting states can exceed the density of hydrostatic equilibrium so that the collapse itself can provide the observed inward motions, ( 3) we consider different equations of state, especially those that are softer than isothermal, and ( 4) we consider dynamic equations of state that are different from the effective equation of state that produces the initial density distribution. This work determines the infall rates over a wide range of parameter space, as characterized by four variables: the initial inward velocity v(infinity), the overdensity Lambda of the initial state, the index Gamma of the static equation of state, and the index gamma of the dynamic equation of state. For the range of parameter space applicable to observed cores, the resulting infall rate is about a factor of 2 larger than that found in previous theoretical studies ( those with hydrostatic initial conditions and v(infinity) = 0). C1 Xavier Univ, Dept Phys, Cincinnati, OH 45207 USA. Univ Michigan, Michigan Ctr Theoret Phys, Dept Phys, Randall Lab 2477, Ann Arbor, MI 48109 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fatuzzo, M (reprint author), Xavier Univ, Dept Phys, 3800 Victory Pkwy, Cincinnati, OH 45207 USA. EM fatuzzo@cerebro.cs.xu.edu; fca@umich.edu; pmyers@cfa.harvard.edu NR 68 TC 53 Z9 53 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 NOV 10 PY 2004 VL 615 IS 2 BP 813 EP 831 DI 10.1086/424656 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300023 ER PT J AU Beuther, H Schilke, P Wyrowski, F AF Beuther, H Schilke, P Wyrowski, F TI High spatial resolution CN and CS observation of two regions of massive star formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : individual (IRAS 20293+3952, IRAS 19217+2336); ISM : molecules; radio lines : ISM; stars : formation; techniques : interferometric ID YOUNG STELLAR OBJECTS; PROTOSTELLAR CANDIDATES; MULTIPLE OUTFLOWS; LINE SURVEY; EMISSION; DISKS; CONTINUUM; SYSTEM; CORES; MASERS AB Molecular line CN, CS, and millimeter continuum observations of two intermediate- to high-mass star-forming regions, IRAS 20293+3952 and IRAS 19410+2336, obtained with the Plateau de Bure Interferometer at high spatial resolution reveal interesting characteristics of the gas and dust emission. In spite of the expectation that the CN and CS morphology might closely follow the dense gas traced by the dust continuum, both molecules avoid the most central cores. Comparing the relative line strengths of various CN hyperfine components, this appears not to be an opacity effect but to be due to chemical and physical effects. The CN data also indicate enhanced emission toward the different molecular outflows in the region. Regarding CS, the emission may avoid the central cores because of high optical depth, but the data also show that the CS emission is nearly always associated with the outflows of the region. Therefore, neither CS nor CN appear well suited for dense gas and disk studies in these two sources, and we recommend the use of different molecules for future massive disk studies. An analysis of the 1 and 3 mm continuum fluxes toward IRAS 20293+3952 reveals that the dust opacity index beta is lower than the canonical value of 2. Tentatively, we identify a decreasing gradient of beta from the edge of the core to the core center. This could be due to increasing optical depth toward the core center and/or grain growth within the densest cores and potential central disks. We detect 3 mm continuum emission toward the collimated outflow emanating from IRAS 20293+3952. The spectral index of alpha similar to 0.8 in this region is consistent with standard models for collimated ionized winds. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu NR 34 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 NOV 10 PY 2004 VL 615 IS 2 BP 832 EP 839 DI 10.1086/424511 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300024 ER PT J AU Wachter, S Patel, SK Kouveliotou, C Bouchet, P Feryal, O Tennant, AF Woods, PM Hurley, K Becker, W Slane, P AF Wachter, S Patel, SK Kouveliotou, C Bouchet, P Feryal, O Tennant, AF Woods, PM Hurley, K Becker, W Slane, P TI Precise localization of the soft gamma repeater SGR 1627-41 and the anomalous X-ray pulsar AXP 1E1841-045 with Chandra SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; infrared : stars; stars : individual (1E 1841-045, SAX J1635.8-4736, SGR 1627-41); stars : neutron; X-rays : stars ID MAGNETIZED NEUTRON-STARS; SUPERNOVA REMNANT G27.4+0.0; NEAR-INFRARED COUNTERPART; TELESCOPE OBSERVATIONS; OPTICAL COUNTERPART; 1E 2259+586; DISCOVERY; DISTANCE; 2MASS; SEARCH AB We present precise localizations of AXP 1E1841-045 and SGR 1627-41 with Chandra. We obtained new infrared observations of SGR 1627-41 and reanalyzed archival observations of AXP 1E1841-045 in order to refine their positions and search for infrared counterparts. A faint source is detected inside the error circle of AXP 1E1841-045. In the case of SGR 1627-41, several sources are located within the error radius of the X-ray position, and we discuss the likelihood of one of them being the counterpart. We compare the properties of our candidates to those of other known anomalous X-ray pulsar (AXP) and soft gamma repeater (SGR) counterparts. We find that the counterpart candidates for SGR 1627-41 and SGR 1806-20 would have to be intrinsically much brighter than AXPs in order to have counterparts detectable with the observational limits currently available for these sources. To confirm the reported counterpart of SGR 1806-20, we obtained new infrared observations during the 2003 July burst activation of the source. No brightening of the suggested counterpart is detected, implying that the counterpart of SGR 1806-20 remains yet to be identified. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM wachter@ipac.caltech.edu; Sandeep.Patel@msfc.nasa.gov; chryssa.kouveliotou@msfc.nasa.gov NR 63 TC 34 Z9 34 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 NOV 10 PY 2004 VL 615 IS 2 BP 887 EP 896 DI 10.1086/424704 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300030 ER PT J AU Zhao, LB Stancil, PC Gu, JP Liebermann, HP Li, Y Funke, P Buenker, RJ Zygelman, B Kimura, M Dalgarno, A AF Zhao, LB Stancil, PC Gu, JP Liebermann, HP Li, Y Funke, P Buenker, RJ Zygelman, B Kimura, M Dalgarno, A TI Radiative charge transfer in collisions of O with He+ SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; stars : individual (SN 1987A); supernovae : general ID CARBON-MONOXIDE; INTERACTION POTENTIALS; LOW-ENERGY; SN 1987A; EXCITATION; SN-1987A; ATOMS; IONS AB Radiative charge transfer has been investigated for collisions of O with He+ with both a fully quantum mechanical theory and an optical potential method. Cross sections and rate coefficients are presented for the process O(P-3) + He+ --> O+(S-4(o), P-2(o),D-2(o)) + He + kw and are compared to those of direct charge transfer. The relative collision energies considered range from 0.1 meV to similar to3 eV with a semiclassical extension to 10 keV and temperatures between 10 and 2.0 x 10(6) K. The results demonstrate that radiative charge transfer is the dominant process over the energy and temperature region considered. Total emission spectra for the two strongest of the ten possible transitions are given for several collision energies, and the origin of resonance-like structures in the spectra is discussed. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Berg Univ Wuppertal, D-42119 Wuppertal, Germany. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Kyushu Univ, Grad Sch Sci, Fukuoka 8128581, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, LB (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM zhao@physast.uga.edu; stancil@physast.uga.edu; buenker@uni-wuppertal.de; bernard@physics.unlv.edu; mineoscc@mbox.nc.kyushu-u.ac.jp; adalgarno@cfa.harvard.edu NR 30 TC 24 Z9 24 U1 0 U2 10 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 NOV 10 PY 2004 VL 615 IS 2 BP 1063 EP 1072 DI 10.1086/424729 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GT UT WOS:000225046300046 ER PT J AU Hwang, U Laming, JM Badenes, C Berendse, F Blondin, J Cioffi, D DeLaney, T Dewey, D Fesen, R Flanagan, KA Fryer, CL Ghavamian, P Hughes, JP Morse, JA Plucinsky, PP Petre, R Pohl, M Rudnick, L Sankrit, R Slane, PO Smith, RK Vink, J Warren, JS AF Hwang, U Laming, JM Badenes, C Berendse, F Blondin, J Cioffi, D DeLaney, T Dewey, D Fesen, R Flanagan, KA Fryer, CL Ghavamian, P Hughes, JP Morse, JA Plucinsky, PP Petre, R Pohl, M Rudnick, L Sankrit, R Slane, PO Smith, RK Vink, J Warren, JS TI A million second Chandra view of Cassiopeia A SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernova remnants; supernovae : general; X-rays : individual (Cassiopeia A); X-rays : ISM ID GAMMA-RAY BURSTS; X-RAY; CAS-A; EXPANSION; COLLAPSE; EJECTA; CORE; NUCLEOSYNTHESIS; PROGENITORS; SUPERNOVAE AB We introduce a million second observation of the supernova remnant Cassiopeia A with the Chandra X-Ray Observatory. The bipolar structure of the Si-rich ejecta (northeast jet and southwest counterpart) is clearly evident in the new images, and their chemical similarity is confirmed by their spectra. These are most likely due to jets of ejecta as opposed to cavities in the circumstellar medium, since we can reject simple models for the latter. The properties of these jets and the Fe-rich ejecta will provide clues to the explosion of Cas A. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. USN, Res Lab, Washington, DC 20375 USA. Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. USN, Res Lab, Washington, DC 20375 USA. N Carolina State Univ, Raleigh, NC 27695 USA. George Washington Univ, Washington, DC 20052 USA. Univ Minnesota, Minneapolis, MN 55455 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Dartmouth Coll, Hanover, NH 03755 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. Arizona State Univ, Tempe, AZ 85287 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Iowa State Univ, Ames, IA 50011 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM hwang@milkyway.gsfc.nasa.gov; jlaming@ssd5.nrl.navy.mil; badenes@ieec.fcr.es; fberendse@ssd5.nrl.navy.mil; john_blondin@ncsu.edu; professor@cioffi.us; tdelaney@astro.umn.edu; dd@space.mit.edu; fesen@snr.dartmouth.edu; kaf@space.mit.edu; fryer@lanl.gov; parviz@pha.jhu.edu; jackph@physics.rutgers.edu; jon.morse@asu.edu; plucinsk@head.cfa.harvard.edu; rob@milkyway.gsfc.nasa.gov; mkp@iastate.edu; larry@astro.umn.edu; ravi@pha.jhu.edu; slane@head.cfa.harvard.edu; rsmith@milkyway.gsfc.nasa.gov; j.vink@sron.nl; jesawyer@physics.rutgers.edu NR 29 TC 117 Z9 118 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 NOV 10 PY 2004 VL 615 IS 2 BP L117 EP L120 DI 10.1086/426186 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870GW UT WOS:000225046600014 ER PT J AU Dumbacher, JP Wako, A Derrickson, SR Samuelson, A Spande, TF Daly, JW AF Dumbacher, JP Wako, A Derrickson, SR Samuelson, A Spande, TF Daly, JW TI Melyrid beetles (Choresine): A putative source for the batrachotoxin alkaloids found in poison-dart frogs and toxic passerine birds SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Pitohui; Ifrita; Phyllobates; APC; mass spectrometry; dietary arthropods ID HOMOBATRACHOTOXIN; DENDROBATIDAE; DEFENSE; ANTS; SKIN AB Batrachotoxins are neurotoxic steroidal alkaloids first isolated from a Colombian poison-dart frog and later found in certain passerine birds of New Guinea. Neither vertebrate group is thought to produce the toxins de novo, but instead they likely sequester them from dietary sources. Here we describe the presence of high levels of batrachotoxins in a little-studied group of beetles, genus Choresine (family Melyridae). These small beetles and their high toxin concentrations suggest that they might provide a toxin source for the New Guinea birds. Stomach content analyses of Pitohui birds revealed Choresine beetles in the diet, as well as numerous other small beetles and arthropods. The family Melyridae is cosmopolitan, and relatives in Colombian rain forests of South America could be the source of the batrachotoxins found in the highly toxic Phyllobates frogs of that region. C1 Smithsonian Conservat Res Ctr, Front Royal, VA 22630 USA. Calif Acad Sci, Dept Birds & Mammals, San Francisco, CA 94103 USA. Bernice P Bishop Museum, Honolulu, HI 96813 USA. NIDDK, Bioorgan Chem Lab, Natl Inst Hlth, Dept Hlth & Human Serv, Bethesda, MD 20892 USA. RP Dumbacher, JP (reprint author), Smithsonian Conservat Res Ctr, Front Royal, VA 22630 USA. EM jdumbacher@calacademy.org NR 19 TC 75 Z9 80 U1 5 U2 39 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 NOV 9 PY 2004 VL 101 IS 45 BP 15857 EP 15860 DI 10.1073/pnas.0407197101 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 872GX UT WOS:000225196800008 PM 15520388 ER PT J AU Osman, RW Whitlatch, RB AF Osman, RW Whitlatch, RB TI The control of the development of a marine benthic community by predation on recruits SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Anachis; ascidians; Botrylloides; Botryllus; bryozoans; dispersal; epifauna; Long Island Sound; marine benthic invertebrates; Mitrella; predation; recruitment ID EARLY POSTSETTLEMENT MORTALITY; SUBTIDAL SOLITARY ASCIDIANS; ROCKY INTERTIDAL COMMUNITY; CRAB CARCINUS-MAENAS; MYTILUS-EDULIS-L; NEW-ENGLAND; POPULATION REGULATION; PELAGIC LARVAE; TAUTOGOLABRUS-ADSPERSUS; BIOLOGICAL DISTURBANCE AB Recruitment is an important process in regulating many marine benthic communities and many studies have examined factors controlling the dispersal and distribution of larval immigrants. However, benthic species also have early post-settlement life-stages that are dramatically different from adult and larval stages. Predation on these stages potentially impacts measured recruitment and the benthic populations and communities that ultimately develop. We examined the consequences of post-settlement predation on 1-day-old to 1-month-old recruits of sessile invertebrates at two field sites in southern New England. One site (Breakwater) was in a protected area with few predators and the other (Pine Island) was < 1 km away in an open coast area with three different predator guilds: small and large invertebrates and fish. The Breakwater site had been dominated for > 10 years by colonial and solitary ascidians. These species were absent from the Pine Island site which was dominated by bryozoans. Our goal was to examine whether post-settlement predation influenced the development and subsequent structure of the epifaunal community. Here we examine long-term changes in community development resulting from post-settlement predation, and contrast these results to those of earlier experiments examining the reductions in observed recruitment by post-settlement predation. Our first long-term experiment examined natural community development at the two sites and whether transplanted communities changed when exposed to the different levels of predation at these sites. The communities that developed at both sites were consistently different from each other and similar to resident communities at their respective sites. On panels transplanted from the Breakwater to Pine Island, solitary ascidians and the colonial ascidian, Botryllus schlosseri, suffered high mortalities on both caged and uncaged treatments, indicative of predation by small predators that could enter cages. Some solitary ascidians did survive inside cages and the colonial ascidian, Botrylloides violaceus, became dominant on all transplanted treatments. On panels transplanted from Pine Island to the Breakwater, ascidians invaded and dominated all treatments except those that were originally caged at Pine Island. In the second long-term experiment, natural communities were allowed to develop on panels exposed at the Breakwater for 1, 2, 3, and 4 weeks. Each set was transplanted to three treatments at Pine Island: open uncaged pilings, caged pilings to exclude fish and large invertebrates, and racks suspended above the bottom to exclude all predators. When 1-week-old communities were transplanted, after 2-3 weeks only bryozoans were found on the open and caged pilings, while colonial ascidians dominated the suspended rack treatment. When older 2-week-old communities were transplanted, colonial ascidians also became dominant in the caged piling treatment and when 3- and 4-week-old communities were transplanted colonial ascidians dominated all three treatments. Solitary ascidians were never abundant on open pilings exposed to fish and large benthic invertebrate predators. Post-settlement predator-prey interactions involved newly settled and juvenile life-stages of a variety of prey species and many invertebrate and vertebrate predator species. The effects of these interactions on recruitment did result in differences in the development and eventual species composition of the communities, even though predators had little if any effect on the adults of the prey species. (C) 2004 Elsevier B.V. All rights reserved. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. RP Osman, RW (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM Osmanr@si.edu NR 93 TC 97 Z9 102 U1 4 U2 61 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD NOV 5 PY 2004 VL 311 IS 1 BP 117 EP 145 DI 10.1016/j.jembe.2004.05.001 PG 29 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 861UN UT WOS:000224444200009 ER PT J AU Huntington, H Callaghan, T Fox, S Krupnik, I AF Huntington, H Callaghan, T Fox, S Krupnik, I TI Matching traditional and scientific observations to detect environmental change: A discussion on Arctic terrestrial ecosystems SO AMBIO LA English DT Article ID ECOLOGICAL KNOWLEDGE; CLIMATE-CHANGE; GLOBAL CHANGE; RESPONSES AB Recent environmental changes are having, and are expected to continue to have, significant impacts in the Arctic as elsewhere in the world. Detecting those changes and determining the mechanisms that cause them are far from trivial problems. The use of multiple methods of observation can increase confidence in individual observations, broaden the scope of information available about environmental change, and contribute to insights concerning mechanisms of change. In this paper, we examine the ways that using traditional ecological knowledge (TEK) together with scientific observations can achieve these objectives. A review of TEK observations in comparison with scientific observations demonstrates the promise of this approach, while also revealing several challenges to putting it into practice on a large scale. Further efforts are suggested, particularly in undertaking collaborative projects designed to produce parallel observations that can be readily compared and analyzed in greater detail than is possible in an opportunistic sample. C1 Abisco Sci Res Stn, SE-98107 Abisco, Sweden. Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Museum Nat Hist, Arctic Studies Ctr, Washington, DC 20560 USA. RP Huntington, H (reprint author), 23834 Clearing Dr, Eagle River, AK 99577 USA. EM hph@alaska.net; terry.callaghan@ans.kiruna.se; sgearh@fas.harvard.edu; krupnik.igor@nmnh.si.edu RI Callaghan, Terens/N-7640-2014 NR 40 TC 41 Z9 44 U1 4 U2 26 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0044-7447 J9 AMBIO JI Ambio PD NOV PY 2004 SU 13 BP 18 EP 23 PG 6 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 870LN UT WOS:000225058700004 ER PT J AU Keita, SOY AF Keita, SOY TI Exploring northeast African metric craniofacial variation at the individual level: A comparative study using principal components analysis SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Article ID Y-CHROMOSOME; HUMAN-POPULATIONS; MIGRATORY EVENTS; POLYMORPHISMS; MIGRATIONS; HAPLOTYPES; ORIGINS; LEVANT; LOCUS; RACE AB A principal components analysis was carried out on male crania from the northeast quadrant of Africa and selected European and other African series. Individuals, not predefined groups, were the units of study, while nevertheless keeping group membership in evidence. The first principal component seems to largely capture "size" variation in crania from all of the regions. The same general morphometric trends were found to exist within the African and European crania, although there was some broad separation along a cline. Anatomically, the second principal component captures predominant trends denoting a broader to narrower nasal aperture combined with a similar shape change in the maxilla, an inverse relation between face-base lengths ("projection") and base breadths, and a decrease in anterior base length relative to base breadth. The third principal component broadly describes trends within Africa and Europe: specifically, a change from a combination of a relatively narrower face and longer vault, to one of a wider face and shorter vault; it shows the northeast quadrant Africans along a cline with the other Africans. Stated in relative terms, the northeastern Africans tend to exhibit narrower bases in relationship to more projecting faces, and broader nasal areas than Europeans, although there is range of variation. Relative to the other African groups, they have narrower nasal areas and narrower faces in relationship to vault length. The crania from the northeast quadrant of Africa collectively demonstrate the greatest pattern of overlap with both Europeans and other Africans. Variation was found to be high in all series but greatest in the African material as a whole. Individuals from different geographical regions frequently plotted near each other, revealing aspects of variation at the level of individuals that is obscured by concentrating on the most distinctive facial traits once used to construct "types" The high level of African interindividual variation in craniometric pattern is reminiscent of the great level of molecular diversity found in Africa. These results, coupled with those of Y chromosome studies, may help generate hypotheses concerning the length of time over which recent craniometric variation emerged in Africa. (C) 2004 Wiley-Liss, Inc. C1 Howard Univ, Natl Human Genome Ctr, Dept Anthropol, Smithsonian Inst, Washington, DC 20060 USA. RP Keita, SOY (reprint author), Howard Univ, Howard Univ Hosp, Ctr Canc, Natl Human Genome Ctr, 615,2041 Georgia Ave NW, Washington, DC 20060 USA. NR 43 TC 7 Z9 7 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1042-0533 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD NOV-DEC PY 2004 VL 16 IS 6 BP 679 EP 689 DI 10.1002/ajhb.20076 PG 11 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 866LF UT WOS:000224774300006 PM 15495230 ER PT J AU Cranmer, SR AF Cranmer, SR TI New views of the solar wind with the Lambert W function SO AMERICAN JOURNAL OF PHYSICS LA English DT Article ID CORONA; DYNAMICS; MODEL AB This paper presents closed-form analytic solutions to two illustrative problems in solar physics that have been considered not solvable in this way previously. Both the outflow speed and the mass loss rate of the solar wind of plasma particles ejected by the Sun are derived analytically for certain illustrative approximations. The calculated radial dependence of the flow speed applies to both Parker's isothermal solar wind equation and Bondi's equation of spherical accretion. These problems involve the solution of transcendental equations containing products of variables and their logarithms. Such equations appear in many fields of physics and are solvable by use of the Lambert W function, which is briefly described. This paper is an example of how new functions can be applied to existing problems. (C) 2004 American Association of Physics Teachers. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu NR 31 TC 48 Z9 49 U1 0 U2 4 PU AMER ASSOC PHYSICS TEACHERS PI COLLEGE PARK PA ONE PHYSICS ELLIPSE, COLLEGE PARK, MD 20740-3845 USA SN 0002-9505 EI 1943-2909 J9 AM J PHYS JI Am. J. Phys. PD NOV PY 2004 VL 72 IS 11 BP 1397 EP 1403 DI 10.1119/1.1775242 PG 7 WC Education, Scientific Disciplines; Physics, Multidisciplinary SC Education & Educational Research; Physics GA 864RZ UT WOS:000224651900007 ER PT J AU Simmons, RB Pogue, MG AF Simmons, RB Pogue, MG TI Redescription of two often-confused noctuid pests, Copitarsia decolora and Copitarsia incommoda (Lepidoptera : Noctuidae : Cuculliinae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE misidentification; morphology; agriculturally important species AB Members of the genus Copitarsia Hampson (Noctuidae) are widespread pests of many agricultural commodities in Central and South America. Two species, Copitarsia incommoda (Walker) and Copitarsia turbata (Herrich-Schaffer), are of particular concern. This misidentification has affected life history studies, risk assessments, and biological control of these pest species. This article redescribes these species and distinguishes them from each other by using adult morphology. C. turbata is placed as a NEW SYNONYM of Copitarsia decolora (Guenee), Copitarsia margaritella (Dognin) is placed as a junior synonym of C. decolora (REVISED SYNONYM), and Copitarsia hampsoni (Brethes) is designated as a NEW SYNONYM of C. incommoda. C1 Museum Natl Hist Nat, USDA, ARS, Smithsonian Inst,Plant Sci Inst,Systemat Entomol, Washington, DC 20013 USA. RP Simmons, RB (reprint author), Univ N Dakota, Dept Biol, Box 9019, Grand Forks, ND 58202 USA. EM rebecca.simmons@und.nodak.edu NR 25 TC 13 Z9 14 U1 1 U2 6 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD NOV PY 2004 VL 97 IS 6 BP 1159 EP 1164 DI 10.1603/0013-8746(2004)097[1159:ROTONP]2.0.CO;2 PG 6 WC Entomology SC Entomology GA 874EZ UT WOS:000225335000006 ER PT J AU Sobrino, C Montero, O Lubian, LM AF Sobrino, C Montero, O Lubian, LM TI UV-B radiation increases cell permeability and damages nitrogen incorporation mechanisms in Nannochloropsis gaditana SO AQUATIC SCIENCES LA English DT Article; Proceedings Paper CT Conference on Aquatic Resources in Arid Lands CY APR 30-MAY 02, 2003 CL Las Cruces, NM DE flow cytometry; membrane permeability; nitrogen incorporation; PAM fluorescence; ultraviolet radiation ID INDUCED DNA-DAMAGE; ULTRAVIOLET-RADIATION; CHLOROPHYLL FLUORESCENCE; MARINE-PHYTOPLANKTON; EXPOSURE; SENSITIVITY; DIATOMS; REPAIR; EUSTIGMATOPHYCEAE; PHOTOPROTECTION AB This study shows the response of Nannochloropsis gaditana, a marine nannoplanktonic species, exposed to UV radiation for 7 days. PAR, UV-A and UV-B ratios used were within the range likely to be observed in nature, a photoperiod of 12L: 12D was maintained, and light irradiances were modified daily to promote cell acclimation. Growth, pigment content, internal nitrogen and carbon content, and photochemical efficiency using PAM fluorometry were assessed in nutrient replete cultures. Cell size, autofluorescence and cell permeability were analysed by flow cytometry. Results showed a cessation of growth after day 3 and a progressive decrease was observed in F-v/F-m values in cultures exposed to UV-B ( plus UV-A and PAR). Flow cytometry analysis also demonstrated an increase in membrane permeability caused by UV-B damage. Cells that showed an increase in membrane permeability also exhibited a proportional decrease in cellular nitrogen content. The results support the conclusion that UV-B radiation can affect N. gaditana nitrogen incorporation mechanisms by direct damage or indirectly by damage to membrane structure and to the photosynthetic apparatus with resulting effects on energy and reductant demand. In contrast, the presence of UV-A radiation was beneficial to cells exposed to PAR plus UVA when compared to those exposed to only-PAR from day 4. This response resulted in cells with a higher nitrogen content and without changes in membrane permeability. C1 CSIC, Inst Ciencias Marinas Andalucia, ES-11510 Cadiz, Spain. RP Sobrino, C (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM cristina.sobrino@icman.csic.es RI Sobrino, Cristina/J-3534-2012; Montero, Olimpio/L-8263-2014; OI Montero, Olimpio/0000-0002-0241-8756; Sobrino, Cristina/0000-0003-0431-1220 NR 33 TC 37 Z9 38 U1 2 U2 21 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 1015-1621 J9 AQUAT SCI JI Aquat. Sci. PD NOV PY 2004 VL 66 IS 4 BP 421 EP 429 DI 10.1007/s00027-004-0731-8 PG 9 WC Environmental Sciences; Limnology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 868BV UT WOS:000224888400009 ER PT J AU Holland, ST Bersier, D Bloom, JS Garnavich, PM Caldwell, N Challis, P Kirshner, R Luhman, K McLeod, B Stanek, KZ AF Holland, ST Bersier, D Bloom, JS Garnavich, PM Caldwell, N Challis, P Kirshner, R Luhman, K McLeod, B Stanek, KZ TI GRB 021211 as a faint analog of GRB 990123: Exploring the similarities and differences in the optical afterglows SO ASTRONOMICAL JOURNAL LA English DT Article DE gamma rays : bursts ID GAMMA-RAY BURST; 28 FEBRUARY 1997; SUPERNOVA 2003DH; ENERGY-RELEASE; STAR-FORMATION; LIGHT CURVES; GRB 990123; EMISSION; VARIABILITY; PHOTOMETRY AB We present BVR(C)JHK(s) photometry of the optical afterglow of the gamma-ray burst GRB 021211 taken at the Magellan, MMT, and WIYN observatories between 0.7 and 50 days after the burst. We find an intrinsic spectral slope at optical and near-infrared wavelengths of 0.69 +/- 0.14 at 0.87 days. The optical decay during the first day is almost identical to that of GRB 990123 except that GRB 021211's optical afterglow was intrinsically approximately 38 times fainter and the transition from the reverse shock to the forward shock may have occurred earlier than it did for GRB 990123. We find no evidence for a jet break or the cooling break passing through optical frequencies during the first day after the burst. There is weak evidence for a break in the J-band decay between 0.89 and 1.87 days, which may be due to a jet. The optical and infrared data are consistent with a relativistic fireball where the shocked electrons are in the slow cooling regime and the electron index is 2.3 +/- 0.1. The forward shock appears to have been expanding in a homogeneous ambient medium during the first day after the burst. Our analysis suggests that the jet of GRB 021211 may have a small opening angle and that the total gamma-ray energy is likely to be much less than the canonical value of 1: 33; 1051 ergs. If this is the case, then it is possible that most of the energy of the burst is in another form such as a frozen magnetic field, supernova ejecta, or a second jet component. The host galaxy of GRB 021211 is subluminous and has a star formation rate of at least 1 M-. yr(-1). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Soc Fellows, Cambridge, MA 02138 USA. RP NASA, Goddard Space Flight Ctr, Code 660-1, Greenbelt, MD 20771 USA. EM sholland@milkyway.gsfc.nasa.gov; bersier@stsci.edu; jbloom@cfa.harvard.edu; pgarnavi@miranda.phys.nd.edu; caldwell@cfa.harvard.edu; pchallis@cfa.harvard.edu; kirshner@cfa.harvard.edu; kluhman@cfa.harvard.edu; bcmcleod@cfa.harvard.edu; kstanek@cfa.harvard.edu NR 55 TC 24 Z9 24 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 NOV PY 2004 VL 128 IS 5 BP 1955 EP 1964 DI 10.1086/425048 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867TX UT WOS:000224866500003 ER PT J AU Ramella, M Boschin, W Geller, MJ Mahdavi, A Rines, K AF Ramella, M Boschin, W Geller, MJ Mahdavi, A Rines, K TI K-band properties of well-sampled groups of galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; infrared : galaxies ID TO-LIGHT RATIOS; INTRACLUSTER PLANETARY-NEBULAE; NEAR-INFRARED PROPERTIES; STELLAR MASS FUNCTIONS; LUMINOSITY FUNCTION; REDSHIFT SURVEY; SPIRAL GALAXIES; VIRGO CLUSTER; RICH CLUSTERS; DIFFUSE LIGHT AB We use a sample of 55 groups and six clusters of galaxies ranging in mass from 7 x 10(11) to 1.5 x 10(15) M-. to examine the correlation of the K-s-band luminosity with mass discovered by Lin and coauthors in 2003. We use the Two-Micron All-Sky Survey catalog and published redshifts to construct complete magnitude-limited redshift surveys of the groups. From these surveys we explore the IR photometric properties of groups members, including their IR color distribution and luminosity function. Although we find no significant difference between the group K-s luminosity function and the general field, there is a difference between the color distribution of luminous group members and their counterparts ( generally background) in the field. There is a significant population of luminous galaxies with H - K-s greater than or similar to 0.35, which are rarely, if ever, members of the groups in our sample. The most luminous galaxies that populate the groups have a very narrow range of IR color. Over the entire mass range covered by our sample, the K-s luminosity increases with mass as L-Ks proportional to M0.64 +/- 0.06, implying that the mass-to-light ratio in the K-s band increases with mass. The agreement between this result and earlier investigations of essentially nonoverlapping sets of systems shows that this window in galaxy formation and evolution is insensitive to the selection of the systems and to the details of the mass and luminosity computations. C1 Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RP Ramella, M (reprint author), Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34131 Trieste, Italy. EM ramella@ts.astro.it; boschin@ts.astro.it; mgeller@cfa.harvard.edu; amahdavi@ifa.hawaii.edu; krines@astro.yale.edu OI Ramella, Massimo/0000-0001-5446-4749 NR 92 TC 28 Z9 32 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 NOV PY 2004 VL 128 IS 5 BP 2022 EP 2036 DI 10.1086/424862 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867TX UT WOS:000224866500008 ER PT J AU Sollins, PK Megeath, ST AF Sollins, PK Megeath, ST TI A near-infrared/millimeter-wave study of six fourth-quadrant high-mass star formation regions SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : stars; ISM : molecules; radio lines : ISM; stars : formation ID H-II REGIONS; MOLECULAR CLOUDS; METHANOL MASERS; POINT SOURCES; DENSE CORES; NGC 6334; NGC-6334; CONTINUUM; GALAXY; G333.6-0.2 AB We present near-infrared and millimeter-wave observations of six high-mass star-forming regions in the fourth quadrant: RCW 108, G333.6, RCW 117, RCW 122, NGC 6334 I, and G351.6. These regions have heliocentric distances of 1.3-3.0 kpc and total luminosities ranging from 0.5 to 3 x 10(5) L-circle dot. Millimeter maps taken in transitions of (CO)-O-18, HC3N, (C16O)-C-12, and SiO with the Swedish-ESO Submillimetre Telescope 15 m telescope detail the structure and kinematics of the clouds. Near-infrared K-band images of the same regions obtained with the MPG/ESO 2.2 m telescope are used to map the stellar surface density. The (CO)-O-18 (1 --> 0) line shows extended high column density gas, with column densities ranging from 10(22) to 3 x 10(23) cm(-2); in contrast, the HC3N ( 15 ! 14) emission shows eight sharply peaked dense cores. We examine these cores for recent and ongoing star formation by searching for high-velocity, non-Gaussian wings on the CO (1 --> 0) and SiO (2 --> 1) lines, peaks in the surface density of stars, and positional coincidences with IRAS point sources, as well as masers and H II regions reported in the literature. All of the cores show evidence of ongoing star formation. NGC 6334 I(N) stands out as a unique case in which an outflow has formed and masers have appeared, but no IRAS source, K-band cluster, or UC H II region has yet appeared; our data support previous claims that this is a rare example of a core in the earliest stages of forming a cluster of high- and low-mass stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sollins, PK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM psollins@cfa.harvard.edu; tmegeath@cfa.harvard.edu NR 42 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2004 VL 128 IS 5 BP 2374 EP 2387 DI 10.1086/425044 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 867TX UT WOS:000224866500030 ER PT J AU Haverkorn, M Katgert, P de Bruyn, AG AF Haverkorn, M Katgert, P de Bruyn, AG TI Properties of the warm magnetized ISM, as inferred from WSRT polarimetric imaging SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic fields; ISM : structure; radio continuum : ISM ID FARADAY-ROTATION; RADIO-EMISSION; MULTIFREQUENCY POLARIMETRY; INTERSTELLAR-MEDIUM; 350 MHZ; GALAXY; FIELD; POLARIZATION; DENSITY; REGION AB We describe a first attempt to derive properties of the regular and turbulent Galactic magnetic field from multi-frequency polarimetric observations of the diffuse Galactic synchrotron background. A single-cell-size model of the thin Galactic disk is constructed which includes random and regular magnetic fields and thermal and relativistic electrons. The disk is irradiated from behind with a uniform partially polarized background. Radiation from the background and from the thin disk is Faraday rotated and depolarized while propagating through the medium. The model parameters are estimated from a comparison with 350 MHz observations in two regions at intermediate latitudes done with the Westerbork Synthesis Radio Telescope. We obtain good agreement between the estimates for the random and regular magnetic field strengths and typical scales of structure in the two regions. The regular magnetic field strength found is a few muG, and the ratio of random to regular magnetic field strength B-ran/B-reg is 0.7 +/- 0.5, for a typical scale of the random component of 15 +/- 10 pc. Furthermore, the regular magnetic field is directed almost perpendicular to the line of sight. This modeling is a potentially powerful method to estimate the structure of the Galactic magnetic field, especially when more polarimetric observations of the diffuse synchrotron background at intermediate latitudes become available. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. ASTRON, NL-7990 AA Dwingeloo, Netherlands. Kapteyn Inst, NL-9700 AV Groningen, Netherlands. RP Haverkorn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl NR 47 TC 17 Z9 17 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 427 IS 1 BP 169 EP U47 DI 10.1051/0004-6361:200400042 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869FP UT WOS:000224969100020 ER PT J AU Haverkorn, M Katgert, P de Bruyn, AG AF Haverkorn, M Katgert, P de Bruyn, AG TI Structure in the polarized Galactic synchrotron emission, in particular "depolarization canals" SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic fields; ISM : structure; radio continuum : ISM ID MAGNETIC-FIELD; MULTIFREQUENCY POLARIMETRY; INTERSTELLAR-MEDIUM; RADIO POLARIZATION; 350 MHZ; REGION; GALAXY; M-51; ISM AB The polarized component of the diffuse radio synchrotron emission of our Galaxy shows structure, which is apparently unrelated to the structure in total intensity, on many scales. The structure in the polarized emission can be due to several processes or mechanisms. Some of those are related to the observational setup, such as beam depolarization-the vector combination and ( partial) cancellation of polarization vectors within a synthesized beam-, or the insensitivity of a synthesis telescope to structure on large scales, also known as the "missing short spacings problem". Other causes for structure in the polarization maps are intrinsic to the radiative transfer of the emission in the warm ISM, which induces Faraday rotation and depolarization. We use data obtained with the Westerbork Synthesis Radio Telescope at 5 frequencies near 350 MHz to estimate the importance of the various mechanisms in producing structure in the linearly polarized emission. In the two regions studied here, which are both at positive latitudes in the second Galactic quadrant, the effect of "missing short spacings" is not important. The properties of the narrow depolarization "canals" that are observed in abundance lead us to conclude that they are mostly due to beam depolarization, and that they separate regions with different rotation measures. As beam depolarization only creates structure on the scale of the synthesized beam, most of the structure on larger scales must be due to depth depolarization. We do not discuss that aspect of the observations here, but in a companion paper we derive information about the properties of the ISM from the structure of the polarized emission. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. ASTRON, NL-7990 AA Dwingeloo, Netherlands. Kapteyn Inst, NL-9700 AV Groningen, Netherlands. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-67, Cambridge, MA 02138 USA. EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl NR 24 TC 28 Z9 28 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 427 IS 2 BP 549 EP 559 DI 10.1051/0004-6361:200400051 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 870LO UT WOS:000225058800014 ER PT J AU Lallement, R Raymond, JC Bertaux, JL Quemerais, E Ko, YK Uzzo, M McMullin, D Rucinski, D AF Lallement, R Raymond, JC Bertaux, JL Quemerais, E Ko, YK Uzzo, M McMullin, D Rucinski, D TI Solar cycle dependence of the helium focusing cone from SOHO/UVCS observations - Electron impact rates and associated pickup ions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE interplanetary medium; Sun : solar wind; Sun : general; plasmas ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; INTERSTELLAR HELIUM; IONIZATION; WIND; HELIOSPHERE; PARAMETERS; EMISSION; HYDROGEN; FLUXES; CLOUD AB The Ultraviolet Coronograph on board SOHO (UVCS) has observed the 58.4 nm glow of the interplanetary He focusing cone at regular intervals since 1996. The intensity decrease with time already observed during the first two years (Michels et al. 2002) has dramatically amplified during the solar activity increase. Intensities seem to reach a plateau in 2001. Using a model of the cone emission which takes into account both photoionization and electron impact ionization of neutral helium we show that the photoionization increase alone cannot explain the observed intensity drop. Data can be fitted if at minimum activity the electron impact ionization rate is the solar cycle average rate predicted by Rucinski & Fahr ( 1989), and if this rate is increased by a factor of about 3.5 between 1996 and 2001. Assuming the Rucinski and Fahr radial dependence, such high electron impact rates create averaged He+ pickup ion (PUI) fluxes which may reach 50% of the fluxes of ions born after photoionization, or 35% of PUI total fluxes, as far as 1 AU from the Sun. In slow and dense solar wind enhancements, in particular in the presence of strong suprathermal tails, PUIs from electron impact could be the dominant species. This could explain a fraction of the observed correlation between He+ and H+ pickups and anticorrelation of He+ fluxes with solar wind velocity. C1 CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. Space Res Ctr, PL-00716 Warsaw, Poland. RP Lallement, R (reprint author), CNRS, Serv Aeron, BP 3, F-91371 Verrieres Le Buisson, France. EM rosine.lallement@aerov.jussieu.fr NR 32 TC 31 Z9 31 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 426 IS 3 BP 867 EP 874 DI 10.1051/0004-6361:200400028 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869FL UT WOS:000224968700014 ER PT J AU Lallement, R Raymond, JC Vallerga, J Lemoine, M Dalaudier, F Bertaux, JL AF Lallement, R Raymond, JC Vallerga, J Lemoine, M Dalaudier, F Bertaux, JL TI Modeling the interstellar-interplanetary helium 58.4 nm resonance glow: Towards a reconciliation with particle measurements SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE interplanetary medium; Sun : solar wind; plasmas; ISM : atoms; ISM : kinematics and dynamics ID EXTREME-ULTRAVIOLET EXPLORER; SOLAR-WIND; HELIOSPHERIC INTERFACE; FOCUSING CONE; EUVE OBSERVATIONS; ELECTRON-DENSITY; SUMER TELESCOPE; WHITE-DWARFS; PICKUP IONS; PARAMETERS AB Pioneering observations of the diffuse HeI-58.4 nm background radiation were performed with a series of satellites in the 70's. Today, their published results on the flow of interstellar helium atoms in the heliosphere are still in contradiction with (i) the results of the particle experiments, i.e. in situ detection of neutrals and pickup ions; (ii) expectations from heliospheric models and comparison with the hydrogen flow; (iii) results of the recent helium glow observations with the Extreme Ultraviolet Explorer (EUVE). Here we discuss these data sets and their modeling, together with the EUVE data and the first coronographic observations of the helium glow obtained with the Ultraviolet Coronographic Spectrometer (UVCS) on board SOHO. We show how they can all be made compatible, and reconciled with in situ data. We have reanalysed the Prognoz data and we derive an updated and higher value of the background noise level. Based on this we can now fit the data satisfactorily with the same set of helium parameters as that one derived from recent EUVE and in situ data. We suggest that other early data sets could be reanalyzed in the same way. Using this updated analysis, EUVE and SOHO-UVCS measurements, we find that all glow data are compatible with the interstellar parameters V-0 approximate to 25 km s(-1), T-0 approximate to 6500 K, lambda(0) approximate to 74.0 deg, beta(0) approximate to 6.0 deg (downwind axis, ecliptic coordinates), as well as with the solar parameters derived from SOHO CELIAS-SEM, SUMER and CDS observations, i. e. the helium photoionisation rate, the 58.4 nm irradiance, and the 58.4 nm Doppler width, found to be between 60 and 90 mAngstrom (30 and 45 km s(-1)). The density is the least constrained parameter from the glow measurements. Prognoz lateral scans, EUVE LWS and SOHO UVCS data are compatible with an interstellar helium density n(0) in the range 0.013-0.016 cm(-3). Prognoz anti-solar data and EUVE scanner data lead to a 40% lower value, suggesting uncertainties in the calibrations. A large part of the contradictions between particle and remote sensing results are thus removed, since the above parameters are very similar to those derived from in situ data. The high electron impact rates inferred from the UVCS remote sensing observations imply high fluxes of newly produced helium pickup ions, which can possibly explain in part the observed correlation between H+ and He+ pickup fluxes, and the inverse correlation between He+ fluxes and solar wind velocity. C1 CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Ecole Polytech, Inst Leprince Ringuet, F-91128 Palaiseau, France. RP CNRS, Serv Aeron, BP 3, F-91371 Verrieres Le Buisson, France. EM rosine.lallement@aerov.jussieu.fr NR 60 TC 51 Z9 51 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 NOV PY 2004 VL 426 IS 3 BP 875 EP 884 DI 10.1051/0004-6361:20035929 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869FL UT WOS:000224968700015 ER PT J AU Mobius, E Bzowski, M Chalov, S Fahr, HJ Gloeckler, G Izmodenov, V Kallenbach, R Lallement, R McMullin, D Noda, H Oka, M Pauluhn, A Raymond, J Rucinski, D Skoug, R Terasawa, T Thompson, W Vallerga, J von Steiger, R Witte, M AF Mobius, E Bzowski, M Chalov, S Fahr, HJ Gloeckler, G Izmodenov, V Kallenbach, R Lallement, R McMullin, D Noda, H Oka, M Pauluhn, A Raymond, J Rucinski, D Skoug, R Terasawa, T Thompson, W Vallerga, J von Steiger, R Witte, M TI Synopsis of the interstellar He parameters from combined neutral gas, pickup ion and UV scattering observations and related consequences SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE interplanetary medium; ISM : general; ISM : atoms; methods : observational; plasmas ID HELIUM FOCUSING CONE; ANOMALOUS COSMIC-RAYS; LYMAN-ALPHA; SOLAR-WIND; TERMINATION SHOCK; HELIOSPHERIC INTERFACE; ULYSSES/GAS-INSTRUMENT; IONIZATION PROCESSES; KINETIC-PARAMETERS; MAGNETIC-FIELD AB A coordinated effort to combine all three methods that are used to determine the physical parameters of interstellar gas in the heliosphere has been undertaken. In order to arrive at a consistent parameter set that agrees with the observations of neutral gas, pickup ions and UV backscattering we have combined data sets from coordinated observation campaigns over three years from 1998 through 2000. The key observations include pickup ions with ACE and Ulysses SWICS, neutral atoms with Ulysses GAS, as well as UV backscattering at the He focusing cone close to the Sun with SOHO UVCS and at 1 AU with EUVE. For the first time also the solar EUV irradiance that is responsible for photo ionization was monitored with SOHO CELIAS SEM, and the He I 58.4 nm line that illuminates He was observed simultaneously with SOHO SUMER. The solar wind conditions were monitored with SOHO, ACE, and WIND. Based on these data the modeling of the interstellar gas and its secondary products in the heliosphere has resulted in a consistent set of interstellar He parameters with much reduced uncertainties, which satisfy all observations, even extended to earlier data sets. It was also established that a substantial ionization in addition to photo ionization, most likely electron impact, is required, with increasing relative importance closer to the Sun. Furthermore, the total combined ionization rate varies significantly with solar latitude, requiring a fully three dimensional and time dependent treatment of the problem. C1 Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland. Russian Acad Sci, Inst Problems Mech, Moscow 117526, Russia. Univ Bonn, Inst Astron & Extraterr Forsch, D-53121 Bonn, Germany. Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Moscow MV Lomonosov State Univ, Dept Mech & Math, Moscow 119899, Russia. ISSI, CH-3012 Bern, Switzerland. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. Natl Astron Observ Japan, Mizusawa, Iwate, Japan. Univ Tokyo, Dept Earth & Planetary Phys, Bunkyo Ku, Tokyo 113, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau 3, Germany. RP Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. EM Eberhard.Moebius@unh.edu RI Von Steiger, Rudolf/F-6822-2011; Thompson, William/D-7376-2012; Izmodenov, Vladislav/K-6073-2012; OI Von Steiger, Rudolf/0000-0002-3350-0023; Izmodenov, Vladislav/0000-0002-1748-0982; Moebius, Eberhard/0000-0002-2745-6978 NR 84 TC 149 Z9 151 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 426 IS 3 BP 897 EP 907 DI 10.1051/0004-6361:20035834 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869FL UT WOS:000224968700017 ER PT J AU Beltran, MT Girart, JM Estalella, R Ho, PTP AF Beltran, MT Girart, JM Estalella, R Ho, PTP TI The dense molecular cores in the IRAS 21391+5802 region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : individual objects : IC1396N; ISM : individual objects : IRAS 21391+5802; ISM : jets and outflows; ISM : molecules; radio lines : ISM; stars : formation ID YOUNG STELLAR OBJECTS; OUTFLOW; ENVELOPE; IC-1396; CLOUD AB We present a detailed kinematical study and modeling of the emission of the molecular cores at ambient velocities surrounding IRAS 21391+5802, an intermediate-mass protostar embedded in IC 1396N. The high-density gas emission is found in association with three dense cores associated with the YSOs BIMA 1, BIMA 2, and BIMA 3. The CS (J = 5 --> 4) and CH3OH (J = 5(-1) --> 4(-1)) emission around BIMA 1 has been modeled by considering a spatially infinitely thin ring seen edge-on by the observer. From the model we find that CS is detected over a wider radii range than CH3OH. A bipolar outflow is detected in the CS (J = 2 --> 1) line centered near BIMA 1. This outflow could be powered by a yet undetected YSO, BIMA 1W, or alternatively could be part of the BIMA 1 molecular outflow. The CS and CH3OH emission associated with the intermediate-mass protostar BIMA 2 is highly perturbed by the bipolar outflow even at cloud velocities, confirming that the protostar is in a very active stage of mass loss. For YSO BIMA 3 the lack of outflow and of clear evidence of infall suggests that both outflow and infall are weaker than in BIMA 1, and that BIMA 3 is probably a more evolved object. C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Barcelona, Dept Astron & Meteorol, Barcelona 08028, Catalunya, Spain. CSIC, IEEC, Inst Ciencies Espai, Barcelona 08034, Catalunya, Spain. RP Beltran, MT (reprint author), Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. EM mbeltran@arcetri.astro.it RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Beltran Sorolla, Maria Teresa/0000-0003-3315-5626 NR 21 TC 14 Z9 14 U1 0 U2 0 PU E D P SCIENCES PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 426 IS 3 BP 941 EP 949 DI 10.1051/0004-6361:20041163 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869FL UT WOS:000224968700020 ER PT J AU Guelin, M Muller, S Cernicharo, J McCarthy, MC Thaddeus, P AF Guelin, M Muller, S Cernicharo, J McCarthy, MC Thaddeus, P TI Detection of the SiNC radical in IRC+10216 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : circumstellar matter; stars : AGB and post-AGB; stars : individual : IRC+10216; ISM : molecules; radio lines : stars ID RATE COEFFICIENTS; LINE SURVEY; ENVELOPE; SILICON AB Following discovery of the free radical SiCN in the C-star envelope IRC+10216, we report the detection in the same source of its isomer SiNC. The microwave spectra of SiNC and SiCN were studied in the laboratory and their rotational transition frequencies are accurately known. The ground fine structure state of SiNC, (2)Pi(1/2), gives rise to a series of rotational transitions, spaced by 12.8 GHz, each with Lambda-doubling. Five weak lines are detected with the IRAM 30-m telescope at the frequencies of the J = 6.5 --> 5.5 (e), 7.5 --> 6.5 (f), 8.5 --> 7.5 (f) and 10.5 --> 9.5 (e) and (f) rotational transitions. Other SiNC lines from these or adjacent rotational transitions are found to be blended with stronger lines from known molecules. The lines assigned to SiNC have a cusped shape, characteristic of species confined to a hollow shell in the outer circumstellar envelope. They are twice weaker than their SiCN counterparts, which have the same shape, and presumably arise in the same region of the envelope. SiNC and SiCN have about the same abundance in IRC+10216, similar to4 x 10(-9) with respect to H-2. This contrasts with HCN, HC3N and HC5N, for which the cyanide to isocyanide abundance ratio is > 100. C1 Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. Inst Estruct Mat, E-28006 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guelin, M (reprint author), Inst Radio Astron Millimetr, 300 Rue Piscine, F-38406 St Martin Dheres, France. EM guelin@iram.fr OI McCarthy, Michael/0000-0001-9142-0008; /0000-0002-9931-1313 NR 16 TC 42 Z9 46 U1 0 U2 1 PU E D P SCIENCES PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2004 VL 426 IS 2 BP L49 EP L52 DI 10.1051/0004-6361:200400074 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869EI UT WOS:000224965800007 ER PT J AU Harris, DE Mossman, AE Walker, RC AF Harris, DE Mossman, AE Walker, RC TI The x-ray jet of 3C 120: Evidence for a nonstandard synchrotron spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (3C 120); galaxies : jets; radiation mechanisms : nonthermal; X-rays : galaxies ID GALACTIC NUCLEI; RADIO JET; 3C 120; EMISSION; COMPTON; MOTIONS; PARSECS; SCALES; HALO AB We report on archival data from the Chandra X-Ray Observatory for the radio jet of 3C 120. We consider the emission process responsible for the X-rays from four knots using spectra constructed from radio, optical, and X-ray intensities. While a simple synchrotron model is adequate for three of the knots, the fourth ("k25''), which was previously detected by ROSAT and is now well resolved with Chandra, still represents a problem for the conventional emission processes. If, as we argue, the flat X-ray spectra from two parts of k25 are synchrotron emission, then it appears that either the emission comes from an electron distribution spectrally distinct from that responsible for the radio emission or at the highest electron energies there is a significant deviation from the power law describing the electron distribution at lower energies. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM harris@cfa.harvard.edu; amossman@cfa.harvard.edu; cwalker@nrao.edu NR 22 TC 29 Z9 29 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 NOV 1 PY 2004 VL 615 IS 1 BP 161 EP 172 DI 10.1086/424442 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800015 ER PT J AU Pfahl, E Loeb, A AF Pfahl, E Loeb, A TI Probing the spacetime around Sagittarius A* with radio pulsars SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy : center; pulsars : general ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; BINARY PULSARS; VELOCITY DISTRIBUTION; RELATIVISTIC GRAVITY; PROPER MOTIONS; NUCLEAR BULGE; MILKY-WAY; GALAXY; SPECTROSCOPY AB The supermassive black hole at the Galactic center harbors a bound cluster of massive stars that should leave neutron star remnants. Extrapolating from the available data, we estimate that similar to1000 radio pulsars may currently orbit Sgr A* with periods of less than or similar to100 yr. Optimistically, 1-10 of the most luminous of these pulsars may be detectable with current telescopes in periodicity searches at frequencies near 10 GHz, where the effects of interstellar scattering are alleviated. Long-term timing observations of such a pulsar would clearly reveal its Keplerian motion and possibly show the effects of relativistic gravity. We briefly discuss how pulsar timing can be used to study the dynamical and interstellar environment of the central black hole and speculate on the prospects for astrometric observations of an orbiting pulsar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pfahl, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM epfahl@cfa.harvard.edu; aloeb@cfa.harvard.edu NR 56 TC 63 Z9 64 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 NOV 1 PY 2004 VL 615 IS 1 BP 253 EP 258 DI 10.1086/423975 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800023 ER PT J AU Korreck, KE Raymond, JC Zurbuchen, TH Ghavamian, P AF Korreck, KE Raymond, JC Zurbuchen, TH Ghavamian, P TI Far Ultravviolet Spectroscopic Explorer observation of the nonradiative collisionless shock in the remnant of SN 1006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (SN 1006); shock waves; supernova remnants; ultraviolet : ISM ID O-VI EMISSION; DIFFUSE INTERSTELLAR-MEDIUM; SUPERNOVA-REMNANTS; SN 1006; OPTICAL-EMISSION; ACCELERATION; NOVA; EQUILIBRATION; SPECTRUM; MODEL AB The appearance of the young supernova remnant SN 1006 is dominated by emission from nonradiative shocks in the northeast and northwest regions. At X-ray energies the northeast shock exhibits predominantly nonthermal synchrotron emission, while the northwest shock exhibits a thermal spectrum. We present far-ultraviolet spectra of the northeast ( NE) and northwest ( NW) portions of SN 1006 acquired with the Far Ultraviolet Spectroscopic Explorer (FUSE). We have detected emission lines of O VI lambdalambda1032, 1038 and broad Lybetalambda1025 in the NW filament but detect no emission lines in the NE region down to a level of 4.7 x 10(-17) ergs cm(-2) s(-1) arcsec(-2). We observed in the NW an O VI intensity of 2.0 +/- 0.2 x 10(-16) ergs cm(-2) s(-1) arcsec(-2) and measured an O VI line width of 2100 +/- 200 km s(-1) at a position where the Halpha width was measured to be 2290 +/- 80 km s(-1). This implies less than mass-proportional heating of the ions. Using the ratio of intensities I(NW)/I(NE)similar ton(NW)/n(NE), the density ratio of the two regions is found to be greater than or equal to4, a value that is consistent with the uncertainties of the ratio of 2.5 measured in 2003 by Long and coworkers. The derived O VI kinetic temperature is compared to previous estimates of electron, proton, and ion temperatures in the remnant to study the relative heating efficiency of various species at the shock front. The degree of postshock temperature equilibration may be crucial to particle acceleration, since the temperature of each species determines the number of high-speed particles available for injection into an acceleration process that could produce Galactic cosmic rays. C1 Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Korreck, KE (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward, Ann Arbor, MI 48109 USA. NR 33 TC 32 Z9 33 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 NOV 1 PY 2004 VL 615 IS 1 BP 280 EP 285 DI 10.1086/424481 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800026 ER PT J AU McClintock, JE Narayan, R Rybicki, GB AF McClintock, JE Narayan, R Rybicki, GB TI On the lack of thermal emission from the quiescent black hole XTE J1118+480: Evidence for the event horizon SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; binaries : close; black hole physics; stars : individual (XTE J1118+480); X-rays : binaries; X-rays : stars ID X-RAY TRANSIENT; ADVECTION-DOMINATED ACCRETION; INTRINSIC MAGNETIC-MOMENTS; SELF-GRAVITATING SYSTEMS; BOSON-FERMION STARS; NEUTRON-STAR; CHANDRA OBSERVATIONS; STRANGE STARS; CEN X-4; MULTIWAVELENGTH OBSERVATIONS AB A soft component of thermal emission is very commonly observed from the surfaces of quiescent, accreting neutron stars. We searched with Chandra for such a surface component of emission from the dynamical black hole candidate XTE J1118+480 (=J1118), which has a primary mass M(1)approximate to8 M-circle dot. None was found, as one would expect if the compact X-ray source is a bona fide black hole that possesses an event horizon. The spectrum of J1118 is well fitted by a simple power-law model that implies an unabsorbed luminosity of L(X)approximate to3.5x10(30) ergs s(-1) (0.3-7 keV). In our search for a thermal component, we fitted our Chandra data to a power-law model (with slope and N-H fixed) plus a series of nine hydrogen atmosphere models with radii ranging from 9/8 to 2.8 Schwarzschild radii. For the more compact models, we included the important effect of self-irradiation of the atmosphere. Because of the remarkably low column density to J1118, N(H)approximate to1.2x10(20) cm(-2), we obtained very strong limits on a hypothetical thermal source: kT(infinity)<0.011 keV and L-infinity,L-th<9.4x10(30) ergs s(-1) (99% confidence level). In analogy with neutron stars, there are two possible sources of thermal radiation from a hypothetical surface of J1118: deep crustal heating and accretion. The former mechanism predicts a thermal luminosity that exceeds the above luminosity limit by a factor of greater than or similar to 25, which implies that either one must resort to contrived models or, as we favor, J1118 is a true black hole with an event horizon. In addition to neutron stars, we also consider emission from several exotic models of compact stars that have been proposed as alternatives to black holes. As we have shown previously, accreting black holes in quiescent X-ray binaries are very much fainter than neutron stars. One potential explanation for this difference is the larger and hence cooler surface of an 8 M-circle dot compact object that might be masked by the interstellar medium. However, our upper limit on the total luminosity of J1118 of 1.3x10(31) ergs s(-1) is far below the luminosities observed for neutron stars. This result strengthens our long-held position that black holes are faint relative to neutron stars because they possess an event horizon. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jem@cfa.harvard.edu; rnarayan@cfa.harvard.edu; grybicki@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 102 TC 62 Z9 62 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 NOV 1 PY 2004 VL 615 IS 1 BP 402 EP 415 DI 10.1086/424474 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800038 ER PT J AU Ghosh, H DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Salim, S Abe, F Bennett, DP Bond, IA Eguchi, S Furuta, Y Hearnshaw, JB Kamiya, K Kilmartin, PM Kurata, Y Masuda, K Matsubara, Y Muraki, Y Noda, S Okajima, K Rattenbury, NJ Sako, T Sekiguchi, T Sullivan, DJ Sumi, T Tristram, PJ Yanagisawa, T Yock, PCM Udalski, A Soszynski, I Wyrzykowski, X Kubiak, M Szymanski, MK Pietrzynski, G Szewczyk, O Zebrun, K Albrow, MD Beaulieu, JP Caldwell, JAR Cassan, A Coutures, C Dominik, M Donatowicz, J Fouque, P Greenhill, J Hill, K Horne, K Jorgensen, UG Kane, S Kubas, D Martin, R Menzies, J Pollard, KR Sahu, KC Wambsganss, J Watson, R Williams, A AF Ghosh, H DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Salim, S Abe, F Bennett, DP Bond, IA Eguchi, S Furuta, Y Hearnshaw, JB Kamiya, K Kilmartin, PM Kurata, Y Masuda, K Matsubara, Y Muraki, Y Noda, S Okajima, K Rattenbury, NJ Sako, T Sekiguchi, T Sullivan, DJ Sumi, T Tristram, PJ Yanagisawa, T Yock, PCM Udalski, A Soszynski, I Wyrzykowski, X Kubiak, M Szymanski, MK Pietrzynski, G Szewczyk, O Zebrun, K Albrow, MD Beaulieu, JP Caldwell, JAR Cassan, A Coutures, C Dominik, M Donatowicz, J Fouque, P Greenhill, J Hill, K Horne, K Jorgensen, UG Kane, S Kubas, D Martin, R Menzies, J Pollard, KR Sahu, KC Wambsganss, J Watson, R Williams, A CA MuFUN Collaboration MOA Collaboration OGLE Collaboration PLANET Collaboration TI Potential direct single-star mass measurement SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; gravitational lensing; stars : fundamental parameters ID GRAVITATIONAL LENSING EXPERIMENT; LARGE-MAGELLANIC-CLOUD; PARALLAX MICROLENS DEGENERACY; SPACE-INTERFEROMETRY-MISSION; DIFFERENCE IMAGE-ANALYSIS; GALACTIC BULGE; EVENT; HALO; EXTINCTION; PHOTOMETRY AB We analyze the light curve of the microlensing event OGLE-2003-BLG-175/MOA-2003-BLG-45 and show that it has two properties that, when combined with future high-resolution astrometry, could lead to a direct, accurate measurement of the lens mass. First, the light curve shows clear signs of distortion due to the Earth's accelerated motion, which yields a measurement of the projected Einstein radius (r) over tilde (E). Second, from precise astrometric measurements, we show that the blended light in the event is coincident with the microlensed source to within about 15 mas. This argues strongly that this blended light is the lens and hence opens the possibility of directly measuring the lens-source relative proper motion mu(rel) and so the mass M=(c(2)/4G)mu(rel)t(E)(r) over tilde (E), where t(E) is the measured Einstein timescale. While the light-curve-based measurement of (r) over tildeE is, by itself, severely degenerate, we show that this degeneracy can be completely resolved by measuring the direction of proper motion mu(rel). C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Dept Astron, Pasadena, CA 91025 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. Korea Astron Obser, Taejon 305348, South Korea. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Nagoya Univ, Solarterr Environm Lab, Nagoya, Aichi 4648601, Japan. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Univ Edinburgh, Astron Inst, Edinburgh EH9 3HJ, Midlothian, Scotland. Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. Natl Astron Observ Japan, Tokyo 1818588, Japan. Univ Auckland, Dept Phys, Auckland, New Zealand. Univ Victoria, Sch Chem & Phys Sci, Wellington, New Zealand. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Natl Aerosp Lab, Tokyo 1828522, Japan. Univ Warsaw Observ, PL-00478 Warsaw, Poland. Univ Concepcion, Dept Fis, Concepcion, Chile. Univ Canterbury, Dept Phys & Astron, Christchurch 4800, New Zealand. Inst Astrophys, F-75014 Paris, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. CEA Saclay, DSM DAPNIA, F-91191 Gif Sur Yvette, France. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria. Observ Midi Pyrenees, UMR 5572, F-31400 Toulouse, France. Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. Astronom Observ, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. Univ Potsdam, D-14469 Potsdam, Germany. Perth Observ, Perth, WA 6076, Australia. S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM ghosh@astronomy.ohio-state.edu; depoy@astronomy.ohio-state.edu; avishay@astro.caltech.du; sgaudi@cfa.harvard.edu; gould@astronomy.ohio-state.edu; cheongho@astroph.chungbuk.ac.kr; yiftah@wise.tau.ac.il; dani@wise.tau.ac.il; eran@wise.tau.ac.il; bgpark@boao.re.kr; pogge@astronomy.ohio-state.edu; abe@stelab.nagoya-u.ac.jp; bennett@emu.phys.nd.edu; iab@roe.ac.uk; sado@stelab.nagoya-u.ac.jp; furuta@stelab.nagoya-u.ac.jp; john.hearnshaw@canterbury.ac.nz; kkamiya@stelab.nagoya-u.ac.jp; pam.kilmartin@canterbury.ac.nz; kurata@stelab.nagoya-u.ac.jp; kmasuda@stelab.nagoya-u.ac.jp; ymatsu@stelab.nagoya-u.ac.jp; muraki@stelab.nagoya-u.ac.jp; sachi.t.noda@nao.ac.jp; okajima@stelab.nagoya-u.ac.jp; nrat001@phy.auckland.ac.nz; sako@stelab.nagoya-u.ac.jp; sekiguchi@stelab.nagoya-u.ac.jp; denis.sullivan@vuw.ac.nz; sumi@astro.princeton.edu; paulonieka@hotmail.com; tyanagi@nal.go.jp; p.yock@auckland.ac.nz; udalski@astrouw.edu.pl; soszynsk@astrouw.edu.pl; wyrzykow@astrouw.edu.pl; mk@astrouw.edu.pl; msz@astrouw.edu.pl; pietrzyn@astrouw.edu.pl; szewczyk@astrouw.edu.pl; zebrun@astrouw.edu.pl; md35@st-andrews.ac.uk RI Gaudi, Bernard/I-7732-2012; Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013; Williams, Andrew/K-2931-2013; OI Williams, Andrew/0000-0001-9080-0105; Dominik, Martin/0000-0002-3202-0343; Salim, Samir/0000-0003-2342-7501 NR 47 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2004 VL 615 IS 1 BP 450 EP 459 DI 10.1086/423665 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800043 ER PT J AU Bensch, F Bergin, EA AF Bensch, F Bergin, EA TI The pure rotational line emission of ortho-water vapor in comets. I. Radiative transfer model SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : general; comets : individual (C/1999 T1); methods : numerical; radiative transfer; radio lines : solar system; submillimeter ID WAVE-ASTRONOMY-SATELLITE; C/1999 H1 LEE; HALE-BOPP; B2 HYAKUTAKE; RADIO TELESCOPES; SUBMILLIMETER; P/HALLEY; ODIN; O1; THERMODYNAMICS AB We present a numerical model for the simulation of water line emission in cometary coma. The model is based on a spherically symmetric density distribution with a constant expansion velocity (Haser model) and the Monte Carlo radiative transfer code published by Hogerheijde & van der Tak. It includes the seven lowest rotational levels of ortho-water, which are the primarily populated levels in the rotationally cold gas of the coma. We discuss the main excitation mechanisms for ortho-water in the coma and study their relative contribution as a function of distance from the comet nucleus. The model is used to derive the water production rate from observations made with the Submillimeter Wave Astronomy Satellite toward comet C/1999 T1 (McNaught-Hartley). They differ from the water production rates derived with an independent model by less than 20% and thus agree within the larger uncertainty due to the limited signal-to-noise ratio of the observations. We give predictions for spectral line observations of H2O and (H2O)-O-18 in comets with present and future airborne and space observatories, including ESA's Herschel Space Observatory and the Stratospheric Observatory for Infrared Astronomy (SOFIA). These models cover a range of water vapor production rates (10(27)-10(29) s(-1)) and heliocentric distances (1-3 AU) and demonstrate that water line emission can be easily detected with Herschel. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Bonn, Inst Radioastron, D-53121 Bonn, Germany. RP Bensch, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 65 TC 28 Z9 28 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 NOV 1 PY 2004 VL 615 IS 1 BP 531 EP 544 DI 10.1086/424439 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GB UT WOS:000224760800051 ER PT J AU Elvis, M Risaliti, G Nicastro, F Miller, JM Fiore, F Puccetti, S AF Elvis, M Risaliti, G Nicastro, F Miller, JM Fiore, F Puccetti, S TI An unveiling event in the type 2 active galactic nucleus NGC 4388: A challenge for a parsec-scale absorber SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4388); galaxies : Seyfert; X-rays : galaxies ID SEYFERT-GALAXY NGC-4388; X-RAY OBSERVATIONS; COMPTON REFLECTION; ASCA OBSERVATIONS; COLUMN DENSITIES; VIRGO CLUSTER; EMISSION; QUASARS; TORI; VARIABILITY AB We present two Rossi X-Ray Timing Explorer (RXTE) Proportional Counter Array (PCA) observations of the type 2 Seyfert galaxy NGC 4388 caught in an unusual low X-ray absorption state. The observations were triggered by a detection in the 1.5-3 keV band of the RXTE all-sky monitor. NGC 4388 was found at a somewhat high continuum level [f(2-10 keV) = 8 x 10(-11) ergs cm(-2) s(-1)] and with a column density N-H similar to 3 x 10(22) cm(-2), a factor of similar to10 lower than normal. The second PCA observation, 4 hr later, gave N-H < 2 x 10(21) cm(-2) indicating, at the 3.1 σ level, variability so rapid it puts the absorber on a few 100 Schwarzschild radii scale, similar to the broad emission line region or smaller. This small scale creates difficulties for the parsec-scale obscuring torus paradigm of unified schemes for type 1 and type 2 active galactic nuclei. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Osservatorio Roma, Sede Monteporzio Catone, INAF, I-00040 Rome, Italy. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elvis@cfa.harvard.edu OI Puccetti, Simonetta/0000-0002-2734-7835; Risaliti, Guido/0000-0002-3556-977X; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 36 TC 98 Z9 98 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 NOV 1 PY 2004 VL 615 IS 1 BP L25 EP L28 DI 10.1086/424380 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GD UT WOS:000224761000007 ER PT J AU Schwartz, DA Virani, SN AF Schwartz, DA Virani, SN TI Chandra measurement of the X-ray spectrum of a quasar at z=5.99 SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars : general; quasars : individual (SDSSp J130608.26+035626.3); X-rays : galaxies ID DIGITAL SKY SURVEY; XMM-NEWTON OBSERVATIONS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; BACKGROUND SPECTRUM; LIKELIHOOD RATIO; RADIO-QUIET; Z-SIMILAR-TO-6; DISCOVERY AB We report the first measurement of the X-ray spectrum of the z = 5.99 quasar SDSSp J130608.26 + 035626.3 from a 120 ks observation by the Chandra ACIS- S instrument. Between 0.5 and 7 keV, corresponding to 3.5-49 keV in the quasar rest frame, we find an energy index of 0.86 +/- 0.2, consistent with the typical indices found for radio-quiet quasars at lower redshifts and inconsistent with the index required to match the diffuse X-ray background. We have a weak indication of a redshifted Fe K line. In comparing the counting rate between an earlier short observation and the longer observation reported here, we find evidence for source variability at the 99.9% confidence level. We note that other nearby X-ray sources would bias the measured alpha(ox) = 1.70 by -0.09 if the X-ray flux were determined from within a 60" extraction circle. Our results for the energy index and the alpha(ox) are consistent with no strong evolution in the active galactic nucleus emission mechanism with redshift out to z approximate to 6 and therefore with the picture that massive black holes have already formed less than 1 Gyr after the big bang. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head.cfa.harvard.edu NR 27 TC 10 Z9 10 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 NOV 1 PY 2004 VL 615 IS 1 BP L21 EP L24 DI 10.1086/425994 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 866GD UT WOS:000224761000006 ER PT J AU Gelfand, JD Lazio, TJW Gaensler, BM AF Gelfand, JD Lazio, TJW Gaensler, BM TI A wide-field, low-frequency radio survey of the field of M31. I. Construction and statistical analysis of the source catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies : individual (M31); radio continuum : galaxies; radio continuum : general ID SKY SURVEY; SPECTRUM; GALAXIES; EMISSION; SCALE AB We present here the results of a 325 MHz radio survey of M31, conducted with the A configuration of the Very Large Array. The survey covered an area of 7.6 deg(2), and a total of 405 radio sources between less than or similar to6" and 170" in extent were mapped with a resolution of 6" and a 1 sigma sensitivity of similar to0.6 mJy beam(-1). For each source, its morphological class, major axis theta(M), minor axis theta(m), position angle theta(PA), peak flux I, integrated flux density S, spectral index alpha, and spectral curvature parameter phi were calculated. A comparison of the flux and radial distribution-both in the plane of the sky and in the plane of M31-of these sources with those of the XMM-Newton Large-Scale Structure Survey and Westerbork Northern Sky Survey revealed that a vast majority of sources detected are background radio galaxies. As a result of this analysis, we expect that only a few sources are intrinsic to M31. These sources are identified and discussed in an accompanying paper. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, Res Lab, Washington, DC 20375 USA. RP Gelfand, JD (reprint author), Harvard Smithsonian Ctr Astrophys, MS-10,60 Garden St, Cambridge, MA 02138 USA. EM jgelfand@cfa.harvard.edu; joseph.lazio@nrl.navy.mil; bgaensler@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 14 TC 12 Z9 12 U1 0 U2 2 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 NOV PY 2004 VL 155 IS 1 BP 89 EP 100 DI 10.1086/424446 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 865KC UT WOS:000224700400006 ER PT J AU Wcislo, WT Arneson, L Roesch, K Gonzalez, V Smith, A Fernandez, H AF Wcislo, WT Arneson, L Roesch, K Gonzalez, V Smith, A Fernandez, H TI The evolution of nocturnal behaviour in sweat bees, Megalopta genalis and M-ecuadoria (Hymenoptera : Halictidae): an escape from competitors and enemies? SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE flexibility; nocturnal foraging; parasitism; social pollination ID LASIOGLOSSUM-DUPLEX; NEST SURVIVAL; EYE SIZE; APOIDEA; BATS; POLLINATION; PARKIA; POLLEN; NIGHT; MIMOSOIDEAE AB Evolutionary transitions to dim-light foraging (predawn matinal, crepuscular, nocturnal) have occurred repeatedly in bees, and may be associated with an escape from enemies or competitors. To date, however, little information has been available to test these hypotheses. Here we provide the first detailed information on the nesting behaviour of two species of Neotropical, nocturnal sweat bees, Megalopta genalis and M. ecuadoria (Hymenoptera: Halictidae). Females are facultatively social or solitary, and construct nests in dead wood. Nocturnal foraging behaviour is bimodal. Bees began foraging after sunset (similar to18:30 h) and ceased foraging approximately 1 h later even though nocturnal flowers with pollen were still abundant; a second foraging bout occurred in the predawn morning, which began at similar to04:45 h and ended around sunrise (similar to06:15 h) when diurnal-blooming flowers were abundant. Bees are capable of controlled flight in full light. They utilized pollen from both canopy and understory plant species, which have diurnal or nocturnal pollen anthesis. Megalopta nests are attacked by generalist predators such as ants, as well as the endoparasitic fly Melaloncha sp. nov. (Phoridae), the beetle Macrosaigon gracilis (Rhipophoridae), the parasitic wasp Lophostigina cincta (Mutillidae), and the brood parasite Megalopta byroni (Halictidae). Overall nest survivorship rates were comparable to those for diurnal relatives, but rates of cell parasitism for Megalopta (much less than 5%) were substantially lower than they are for day-flying relatives, offering some support for the hypothesis that the evolution of nocturnal behaviour enables escape from natural enemies. (C) 2004 The Linnean Society of London. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Wcislo, WT (reprint author), STRI, Unit 0948, APO AA, Miami, FL 34002 USA. EM WcisloW@si.edu RI Gonzalez Betancourt, Victor /B-9528-2011; Gonzalez, Victor/B-4072-2015 NR 96 TC 81 Z9 83 U1 2 U2 19 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD NOV PY 2004 VL 83 IS 3 BP 377 EP 387 DI 10.1111/j.1095-8312.2004.00399.x PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 871PU UT WOS:000225146500008 ER PT J AU Greiner, B Ribi, WA Wcislo, WT Warrant, EJ AF Greiner, B Ribi, WA Wcislo, WT Warrant, EJ TI Neural organisation in the first optic ganglion of the nocturnal bee Megalopta genalis SO CELL AND TISSUE RESEARCH LA English DT Article DE visual system; compound eye; first optic ganglion; retinula cell axons; first-order interneurons; spatial summation; Megalopta genalis, nocturnal bee, female (Insecta) ID LAMINA GANGLIONARIS; MONOPOLAR CELLS; FINE-STRUCTURE; HALICTID BEE; SUPERPOSITION; VISION; NIGHT; GOLGI; EYE; ORIENTATION AB Each neural unit (cartridge) in the first optic ganglion (lamina) of the nocturnal bee Megalopta genalis contains nine receptor cell axons (6 short and 3 long visual fibres), and four different types of first-order interneurons, also known as L-fibres (L1 to L4) or lamina monopolar cells. The short visual fibres terminate within the lamina as three different types (svf 1, 2, 3). The three long visual fibres pass through the lamina without forming characteristic branching patterns and terminate in the second optic ganglion, the medulla. The lateral branching pattern of svf 2 into adjacent cartridges is unique for hymenopterans. In addition, all four types of L-fibres show dorso-ventrally arranged, wide, lateral branching in this nocturnal bee. This is in contrast to the diurnal bees Apis mellifera and Lasioglossum leucozonium, where only two out of four L-fibre types (L2 and L4) reach neighbouring cartridges. In M. genalis, L1 forms two sub-types, viz. L1-a and L1-b; L1-b in particular has the potential to contact several neighbouring cartridges. L2 and L4 in the nocturnal bee are similar to L2 and L4 in the diurnal bees but have dorso-ventral arborisations that are twice as wide. A new type of laterally spreading L3 has been discovered in the nocturnal bee. The extensive neural branching pattern of L-fibres in M. genalis indicates a potential role for these neurons in the spatial summation of photons from large groups of ommatidia. This specific adaptation in the nocturnal bee could significantly improve reliability of vision in dim light. C1 Lund Univ, Dept Cell & Organism Biol, S-22362 Lund, Sweden. Univ HUman Sci Principal Liechtenstein, FL-9495 Triesen, Liechtenstein. Smithsonian Trop Res Inst, Balboa, Panama. RP Greiner, B (reprint author), Lund Univ, Dept Cell & Organism Biol, Helgonavagen 3, S-22362 Lund, Sweden. EM birgit.greiner@cob.lu.se NR 28 TC 37 Z9 38 U1 1 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0302-766X EI 1432-0878 J9 CELL TISSUE RES JI Cell Tissue Res. PD NOV PY 2004 VL 318 IS 2 BP 429 EP 437 DI 10.1007/s00441-004-0945-z PG 9 WC Cell Biology SC Cell Biology GA 865VW UT WOS:000224733300014 PM 15365811 ER PT J AU Cavender-Bares, J Kitajima, K Bazzaz, FA AF Cavender-Bares, J Kitajima, K Bazzaz, FA TI Multiple trait associations in relation to habitat differentiation among 17 Floridian oak species SO ECOLOGICAL MONOGRAPHS LA English DT Review DE detrended correspondence analysis; fire regime; functional traits; leaf life span; phylogenetic lineage; Quercus; soil moisture; soil nutrients ID RAIN-FOREST TREES; LEAF LIFE-SPAN; SAND PINE SCRUB; RESOURCE AVAILABILITY; ASYMPTOTIC HEIGHT; TROPICAL FORESTS; DECIDUOUS LEAVES; USE EFFICIENCY; QUERCUS-RUBRA; FIRE REGIME AB Differentiation of species distributions along environmental gradients and phenotypic specialization help explain the co-presence of 17 oak species that might otherwise be expected to competitively exclude one another. In an effort to understand the role of niche differentiation in the co-presence of these congeneric species in north-central Florida, we examined the community structure of oak-dominated forests in this region in relation to environmental variables and a suite of life history and physiological traits. Landscape distribution patterns of oaks and other woody species were determined from randomly established plots in three state parks. Soil moisture, nutrient availability, and fire regime were found to be critical factors influencing community structure, and the distribution of oak species was strongly correlated with these gradients. Detrended correspondence analysis of species' distributions supported the grouping of oak species into three major community types: (1) hammock, (2) sandhill, and (3) scrub. Principal components of multiple traits also supported differentiation of oak species into these three groups. There is clear evidence for ecological sorting among the oaks in these forests as species partition environmental gradients more than expected by chance, and most functional traits of species correspond to species distributions as predicted based on a priori understanding of trait function. Across phylogenetic lineages, species showed evolutionary convergence in function and habitat. preference. In contrast, leaf-level traits were conserved within phylogenetic lineages and were not well correlated with local habitat factors, but rather with the broader geographic distributions and northern range limits of species. The cumulative results reported here provide strong evidence that oak species specialize for particular niches via trade-offs in functional traits, and such niche partitioning contributes to the high diversity of oak species at the landscape level. At smaller spatial scales, phylogenetic diversity among the oaks is likely to be important in promoting their coexistence through other mechanisms. C1 Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Harvard Univ, Dept Organism & Evolut Biol, Sch Med, Cambridge, MA 02138 USA. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. RP Cavender-Bares, J (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Dr, St Paul, MN 55108 USA. EM cavender@umn.edu RI Cavender-Bares, Jeannine/K-5716-2013 NR 113 TC 143 Z9 151 U1 6 U2 69 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9615 J9 ECOL MONOGR JI Ecol. Monogr. PD NOV PY 2004 VL 74 IS 4 BP 635 EP 662 DI 10.1890/03-4007 PG 28 WC Ecology SC Environmental Sciences & Ecology GA 871ZY UT WOS:000225176500005 ER PT J AU Hubbell, SP Borda-De-Agua, L AF Hubbell, SP Borda-De-Agua, L TI The unified neutral theory of biodiversity and biogeography: Reply SO ECOLOGY LA English DT Editorial Material C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, APO, AA 34003 USA. RP Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. EM lbagua@yahoo.co.jp RI Borda-de-Agua, Luis/D-6063-2011 OI Borda-de-Agua, Luis/0000-0002-0802-6235 NR 9 TC 12 Z9 13 U1 5 U2 60 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD NOV PY 2004 VL 85 IS 11 BP 3175 EP 3178 DI 10.1890/04-0808 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 873EW UT WOS:000225263500027 ER PT J AU Novotny, V Miller, SE Leps, J Basset, Y Bito, D Janda, M Hulcr, J Damas, K Weiblen, GD AF Novotny, V Miller, SE Leps, J Basset, Y Bito, D Janda, M Hulcr, J Damas, K Weiblen, GD TI No tree an island: the plant-caterpillar food web of a secondary rain forest in New Guinea SO ECOLOGY LETTERS LA English DT Article DE ecological succession; herbivore communities; host specificity; insect-plant interactions; invasive species; Lepidoptera; Malesia; Papua New Guinea; species richness; tropical forests ID PAPUA-NEW-GUINEA; TROPICAL FOREST; PARASITOID COMMUNITY; PIPER-ADUNCUM; HOST-SPECIFICITY; DIVERSITY; INSECTS; LEPIDOPTERA; HERBIVORES; VEGETATION AB We characterized a plant-caterpillar food web from secondary vegetation in a New Guinean rain forest that included 63 plant species (87.5% of the total basal area), 546 Lepidoptera species and 1679 trophic links between them. The strongest 14 associations involved 50% of all individual caterpillars while some links were extremely rare. A caterpillar randomly picked from the vegetation will, with greater than or equal to 50% probability, (1) feed on one to three host plants (of the 63 studied), (2) feed on < 20% of local plant biomass and (3) have greater than or equal to 90% of population concentrated on a single host plant species. Generalist species were quantitatively unimportant. Caterpillar assemblages on locally monotypic plant genera were distinct, while sympatric congeneric hosts shared many caterpillar species. The partitioning of the plant-caterpillar food web thus depends on the composition of the vegetation. In secondary forest the predominant plant genera were locally monotypic and supported locally isolated caterpillar assemblages. C1 Univ S Bohemia, Inst Entomol, Czech Acad Sci, Ceske Budejovice 37005, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20013 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Papua New Guinea, Dept Biol, Port Moresby, Papua N Guinea. New Guinea Binatang Res Ctr, Madang, Papua N Guinea. Forest Res Inst, Lae, Papua N Guinea. Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Novotny, V (reprint author), Univ S Bohemia, Inst Entomol, Czech Acad Sci, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM novotny@entu.cas.cz RI Leps, Jan/B-6913-2013; Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; Janda, Milan/H-7216-2014; OI Leps, Jan/0000-0002-4822-7429; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 50 TC 45 Z9 46 U1 0 U2 11 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD NOV PY 2004 VL 7 IS 11 BP 1090 EP 1100 DI 10.1111/j.1461-0248.2004.00666.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 861ER UT WOS:000224399400009 ER PT J AU Casas, V Kline, DI Wegley, L Yu, YN Breitbart, M Rohwer, F AF Casas, V Kline, DI Wegley, L Yu, YN Breitbart, M Rohwer, F TI Widespread association of a Rickettsiales-like bacterium with reef-building corals SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID WHITE-BAND DISEASE; HALIOTIS-CRACHERODII; WITHERING-SYNDROME; ACROPORA-PALMATA; BLACK ABALONE; MASS; COMMUNITIES; PROKARYOTES; SPREAD AB White band disease type I (WBD I) has been a major cause of the dramatic decline of Acroporid coral populations throughout the Caribbean during the last two decades, yet the aetiological agent of this disease is unknown. In this study, the bacterial communities associated with both healthy and diseased Acropora species were compared by 16S rDNA analyses. The bacterial communities of both healthy and diseased Acropora spp. were dominated by a single ribotype with 90% identity to a bacterium in the order Rickettsiales. Screening by nested PCR specific to the coral-associated Rickettsiales 1 (CAR1) bacterium showed that this microbe was widespread in both healthy and diseased A. cervicornis and A. palmata corals from 'healthy' (i.e. low WBD I incidence) and 'stressed' reefs (i.e. high WBD I incidence). These results indicate that there were no dramatic changes in the composition of the microbial community associated with WBD I. CAR1 was also associated with non-Acroporid corals of the Caribbean, as well as with two Acroporid corals native to the Pacific. CAR1 was not present in the water column. This bacterium was also absent from preserved Caribbean Acroporid samples collected between 1937 and 1980 before the outbreak of WBD I. These results suggest CAR1 is a relatively new bacterial associate of Acroporids and that a non-bacterial pathogen might be the cause of WBD I. C1 San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. Univ Calif San Diego, 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 forest@sunstroke.sdsu.edu RI Breitbart, Mya/B-1366-2009 OI Breitbart, Mya/0000-0003-3210-2899 FU PHS HHS [5 R25 G58906-05] NR 44 TC 38 Z9 38 U1 0 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD NOV PY 2004 VL 6 IS 11 BP 1137 EP 1148 DI 10.1111/j.1462-2920.2004.00647.x PG 12 WC Microbiology SC Microbiology GA 860MJ UT WOS:000224347400003 PM 15479247 ER PT J AU Doyle, J Friedrich, B Krems, RV Masnou-Seeuws, F AF Doyle, J Friedrich, B Krems, RV Masnou-Seeuws, F TI Quo vadis, cold molecules? SO EUROPEAN PHYSICAL JOURNAL D LA English DT Editorial Material ID BOSE-EINSTEIN CONDENSATE; 2-SPECIES MAGNETOOPTICAL TRAP; SUPERFLUID-HELIUM DROPLETS; STATE POTASSIUM MOLECULES; ULTRACOLD TEMPERATURES; GROUND-STATE; FESHBACH RESONANCES; VIBRATIONAL-RELAXATION; ATOM-MOLECULE; PHOTOASSOCIATIVE SPECTROSCOPY AB `We give a snapshot of the rapidly developing field of ultracold polar molecules and walk the reader through the papers appearing in this Topical Issue. C1 Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Max Planck Gesell, Fritz Haber Inst, D-14195 Berlin, Germany. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. CNRS, Aime Cotton Lab, F-91405 Orsay, France. RP Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. NR 161 TC 344 Z9 347 U1 2 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1434-6060 EI 1434-6079 J9 EUR PHYS J D JI Eur. Phys. J. D PD NOV PY 2004 VL 31 IS 2 BP 149 EP 164 DI 10.1140/epjd/e2004-00151-x PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 882IW UT WOS:000225933600001 ER PT J AU Taylor-Juarros, E Cete, R Kirby, K AF Taylor-Juarros, E Cete, R Kirby, K TI Formation of ultracold polar molecules via Raman excitation SO EUROPEAN PHYSICAL JOURNAL D LA English DT Article ID BOSE-EINSTEIN CONDENSATION; VIBRATIONAL LEVELS; STATE; LIH; LITHIUM; ATOMS; PHOTOASSOCIATION; LIFETIMES; GAS AB Alkali hydride molecules are very polar, exhibiting large ground-state dipole moments. As ultracold sources of alkali atoms, as well as hydrogen, have been created in the laboratory, we explore theoretically the feasibility of forming such molecules from a mixture of the ultracold atomic gases, employing a two-photon stimulated radiative association process - Raman excitation. Using accurate molecular potential energy curves and dipole transition moments, we have calculated the rate coefficients for populating all the vibrational levels of the X(1)Sigma(+) state of LiH via the excited A(1)Sigma(+) state. We have found that significant molecule formation rates can be realized with laser intensities and atomic densities that are attainable experimentally. Because of the large X state dipole moment, rapid cascade occurs down the ladder of vibrational levels to v = 0. The calculated recoil momentum imparted to the molecule is small, and thus negligible trap loss results from the cascade process. This allows for the build-up of a large population of v = 0 trapped molecules. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Taylor-Juarros, E (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. EM eliztj@phys.uconn.edu NR 29 TC 10 Z9 10 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1434-6060 J9 EUR PHYS J D JI Eur. Phys. J. D PD NOV PY 2004 VL 31 IS 2 BP 213 EP 219 DI 10.1140/epjd/e2004-00157-4 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 882IW UT WOS:000225933600007 ER PT J AU Dechmann, DKN Kalko, EKV Kerth, G AF Dechmann, DKN Kalko, EKV Kerth, G TI Ecology of an exceptional roost: energetic benefits could explain why the bat Lophostoma silvicolum roosts in active termite nests SO EVOLUTIONARY ECOLOGY RESEARCH LA English DT Article DE basal metabolic rate; Nasutitermes corniger; roost making; temperature; Tonatia silvicola ID CHALINOLOBUS-TUBERCULATUS; MYOTIS-BECHSTEINII; NEW-ZEALAND; SELECTION; PHYLLOSTOMIDAE; MICROCLIMATE; TEMPERATURE; CHIROPTERA; FIDELITY; RODENTIA AB The ability to create shelters that provide protection from the environment is widespread among animals. However, in spite of the central role roosts play in the life of bats (Chiroptera), only a few species have developed the ability to make their own refuges, one of them being the Neotropical Lophostoma silvicolum. This bat creates and inhabits cavities in active arboreal nests of the termite Nasutitermes corniger. We measured temperature in cavities inside active and dead termite nests. and in tree holes occupied by closely related bats, to determine whether energetic benefits compensate for the cost of excavating the hard nests. The inside temperatures of active termite nests were very stable and 2.1-2.8degreesC warmer than those of the other two potential roost types. The observed temperature difference is estimated to allow euthermic L. silvicolum to save about 5% of their daily energy expenditure when roosting in active termite nests instead of dead nests or tree holes. Suitable roosting conditions result from the presence of termites and are independent of nest architecture. Our results indicate that the benefits of higher temperatures may be one of the driving forces promoting the evolution of active roost making in bats. C1 Univ Zurich Irchel, Inst Zool, CH-8057 Zurich, Switzerland. Univ Ulm, D-89075 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Dechmann, DKN (reprint author), Univ Zurich Irchel, Inst Zool, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM dechmann@zool.unizh.ch RI Dechmann, Dina/A-1827-2010 NR 46 TC 37 Z9 37 U1 3 U2 15 PU EVOLUTIONARY ECOLOGY LTD PI TUCSON PA UNIV ARIZONA, 321 BIOSCIENCES WEST, TUCSON, AZ 85721 USA SN 1522-0613 J9 EVOL ECOL RES JI Evol. Ecol. Res. PD NOV PY 2004 VL 6 IS 7 BP 1037 EP 1050 PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 873DJ UT WOS:000225259300007 ER PT J AU Shepard, MK Benner, LAM Ostro, SJ Campbell, DB Shapiro, II Chandler, JF AF Shepard, MK Benner, LAM Ostro, SJ Campbell, DB Shapiro, II Chandler, JF TI Radar detection of near-Earth Asteroids 1915 Quetzalcoatl, 3199 Nefertiti, 3757 (1982 XB), and 4034 (1986 PA) SO ICARUS LA English DT Article DE asteroids; radar ID MAIN-BELT; OBJECTS; PHOTOMETRY AB We describe Arecibo (2380 MHz, 12.6 cm) Doppler-only radar detections of near-Earth Asteroids 1915 Quetzalcoatl, 3199 Nefertiti, 3757 (1982 XB), and 4034 (1986 PA) obtained between 1981 and 1989. Estimates of the echo spectral bandwidths, radar cross-sections, and circular polarization ratios of these objects constrain their sizes, radar albedos, surface roughnesses, taxonomic classes, rotation periods, and pole directions. Our radar constraints on the diameters of Quetzalcoat1 and Nefertiti are most consistent with sizes determined using thermal-radiometry and the Fast Rotation Model (FRM); this consistency may indicate that these asteroids have surfaces of high thermal inertia (i.e., little or no regolith). Constraints on Quetzalcoatl's radar albedo rule out a "metallic M" classification. The radar constraints for Nefertiti are inconsistent with a rotation pole published by Kaasalainen et al. (2004, Icarus 167, 178). Our estimates of 1982 XB's size are consistent with previously published estimates. The radar bandwidth of 1986 PA places an upper bound of about 24 h on its rotation period. (C) 2004 Elsevier Inc. All rights reserved. C1 Bloomsburg Univ Penn, Dept Geog & Geosci, Bloomsburg, PA 17815 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shepard, MK (reprint author), Bloomsburg Univ Penn, Dept Geog & Geosci, Bloomsburg, PA 17815 USA. EM mshepard@bloomu.edu NR 28 TC 2 Z9 2 U1 0 U2 0 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 NOV PY 2004 VL 172 IS 1 BP 170 EP 178 DI 10.1016/j.icarus.2004.06.003 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 869HK UT WOS:000224973800014 ER PT J AU Parenti, LR Grier, HJ AF Parenti, LR Grier, HJ TI Evolution and phylogeny of gonad morphology in bony fishes SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Patterns and Processes in the Evolution of Fishes CY JAN 04-08, 2003 CL Toronto, CANADA SP Soc Integrat & Comparat Biol ID HALFBEAK GENERA DERMOGENYS; COMMON SNOOK; REPRODUCTIVE-BIOLOGY; OOCYTE GROWTH; TELEOSTEI; HEMIRAMPHIDAE; TESTIS; MATURATION; NOMORHAMPHUS; FLORIDA AB Gonad morphology at the gross anatomical or histological levels has long been studied by fisheries biologists to identify annual reproductive cycles and length of breeding season, among other goals. Comparative surveys across vertebrate taxa have not been detailed enough, however, to describe fully the differences and similarities among gonads of bony fishes and other vertebrates, and to use gonad morphology in phylogenetic systematic analyses. An emerging constant among vertebrates is the presence of a germinal epithelium composed of somatic and germ cells in both males and females. In females, the germinal epithelium lines the ovarian lamellae. In males, arrangement of the germinal epithelium into compartments varies among osteichthyans: basal taxa have an anastomosing tubular testis, whereas derived taxa have a lobular testis. The lobular testis is proposed as a synapomorphy of the Neoteleostei. The annual reproductive cycle is hypothesized to be the source of morphological variation among testis types. Elongation of germinal compartments during early maturation may result in a transition from anastomosing tubular to lobular testes. In all male atherinomorphs surveyed, spermatogonia are restricted to the distal termini of lobules rather than being distributed along the lobule; there is an epithelioid arrangement of Sertoli and germ cells rather than a germinal epithelium. Arrest of the maturation-regression phases is hypothesized to lead to formation of the atherinomorph testis. Atherinomorphs also have a distinctive egg with fluid, rather than granular, yolk. Variation among germinal epithelia is interpreted in a developing phylogenetic framework to understand evolution of gonad morphology and to propose gonad characters for phylogenetic analyses. C1 Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Dept Zoo,Div Fishes, Washington, DC 20013 USA. Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Dept Zoo,Div Fishes, POB 37012, Washington, DC 20013 USA. EM parentil@si.edu NR 74 TC 114 Z9 121 U1 2 U2 18 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD NOV PY 2004 VL 44 IS 5 BP 333 EP 348 DI 10.1093/icb/44.5.333 PG 16 WC Zoology SC Zoology GA 881GJ UT WOS:000225851100002 PM 21676719 ER PT J AU Santini, F Tyler, JC AF Santini, F Tyler, JC TI The importance of even highly incomplete fossil taxa in reconstructing the phylogenetic relationships of the Tetraodontiformes (Acanthomorpha : Pisces) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Patterns and Processes in the Evolution of Fishes CY JAN 04-08, 2003 CL Toronto, CANADA SP Soc Integrat & Comparat Biol ID MISSING DATA; FISHES; OSTRACIIDAE; PARSIMONY AB The use of fossils in the phylogenetics of extant clades traditionally has been a contentious issue. Fossils usually are relatively incomplete, and their use commonly leads to an increase in the number of equally most parsimonious trees and a decrease in the resolution of phylogenies. Fossils alone, however, provide certain kinds of information about the biological history of a clade, and computer simulations have shown that even highly incomplete material can, under certain circumstances, increase the accuracy of a phylogeny, rather than decrease it. Because empirical data are still scarce on the effects of the inclusion of fossils on phylogenetic reconstructions, we attempted to investigate this problem by using a relatively well-known group of acanthomorph fishes, the Tetraodontiformes (triggerfishes, pufferfishes, and ocean sunfishes), for which robust phylogenies using extant taxa already exist and that has a well-studied fossil record. Adding incomplete fossil taxa of tetraodontiforms usually increases the number of equally most parsimonious trees and often decreases the resolution of consensus trees. However, adding fossil taxa may help to correctly establish relationships among lineages that have experienced high degrees of morphological diversification by allowing for a reinterpretation of homologous and homoplastic features, increasing the resolution rather than decreasing it. Furthermore, taxa that were scored for 25% or more of their characters did not cause a significant loss of resolution, while providing unique biological information. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. Univ Toronto, Dept Zool, Toronto, ON M5S 3G5, Canada. RP Santini, F (reprint author), Museum Natl Hist Nat, Dept Syst & Evolut, Case Postale 26,43 Rue Cuvier, F-75231 Paris 05, France. EM fsantini@mnhn.fr NR 42 TC 40 Z9 42 U1 2 U2 7 PU SOC INTEGRATIVE COMPARATIVE BIOLOGY PI MCLEAN PA 1313 DOLLEY MADISON BLVD, NO 402, MCLEAN, VA 22101 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD NOV PY 2004 VL 44 IS 5 BP 349 EP 357 DI 10.1093/icb/44.5.349 PG 9 WC Zoology SC Zoology GA 881GJ UT WOS:000225851100003 PM 21676720 ER PT J AU Lovejoy, NR Iranpour, M Collette, BB AF Lovejoy, NR Iranpour, M Collette, BB TI Phylogeny and jaw ontogeny of beloniform fishes SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Patterns and Processes in the Evolution of Fishes CY JAN 04-08, 2003 CL Toronto, CANADA SP Soc Integrat & Comparat Biol ID NEEDLEFISHES TELEOSTEI; EVOLUTION; EXOCOETIDAE; SYSTEMATICS; HETEROCHRONY; BELONIDAE; DNA AB To investigate jaw evolution in beloniform fishes, we reconstructed the phylogeny of 54 species using fragments of two nuclear (RAG2 and Tmo-4C4) and two mitochondrial (cytochrome b and 16S rRNA) genes. Our total molecular evidence topology refutes the monophyly of needlefishes (Belonidae) and half-beaks (Hemiramphidae), but supports the monophyly of flyingfishes (Exocoetidae) and sauries (Scomberesocidae). Flyingfishes are nested within halfbeaks, and sauries are nested within needlefishes. Optimization of jaw characters on the tree reveals a diverse array of evolutionary changes in ontogeny. During their development, needlefishes pass through a "halfbeak" stage that closely resembles the adult condition in the hemiramphid halfbeaks. The reconstruction of jaw transitions falsifies the hypothesis that halfbeaks are paedomorphic derivatives of needlefishes. Instead, halfbeaks; make up a basal paraphyletic grade within beloniforms, and the needlefish jaw morphology is relatively derived. The parallel between needlefish ontogeny and beloniform phylogeny is discussed, and clades amenable to future morphological analysis are proposed. C1 Univ Manitoba, Dept Zool, Winnipeg, MB R3T 2N2, Canada. Smithsonian Inst, Natl Marine Fisheries Serv, Systemat Lab, Washington, DC 20013 USA. RP Lovejoy, NR (reprint author), Univ Manitoba, Dept Zool, Z320 Duff Roblin Bldg, Winnipeg, MB R3T 2N2, Canada. EM nate_lovejoy@umanitoba.ca NR 40 TC 30 Z9 33 U1 1 U2 7 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD NOV PY 2004 VL 44 IS 5 BP 366 EP 377 DI 10.1093/icb/44.5.366 PG 12 WC Zoology SC Zoology GA 881GJ UT WOS:000225851100005 PM 21676722 ER PT J AU Skog, JE Mickel, JT Moran, RC Volovsek, M Zimmer, EA AF Skog, JE Mickel, JT Moran, RC Volovsek, M Zimmer, EA TI Molecular studies of representative species in the fern genus Elaphoglossum (Dryopteridaceae) based on cpDNA sequences rbcL, trnL-F, and rps4-trnS SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE molecular systematics; chloroplast genes; Pteridophyta; ferns; Dryopteridaceae; Elaphoglossum ID PHYLOGENETIC ANALYSIS; NUCLEOTIDE-SEQUENCES; DNA-SEQUENCES; MORPHOLOGY AB Phylogenetic relationships among 48 species representing the nine sections within the fern genus Elaphoglossum were investigated using cpDNA sequence data from rbcL, trnL-F, and rps4-trnS. Elaphoglossum is shown to be a well-supported, monophyletic genus containing five major clades. Mapping of morphological characters onto the molecular phylogeny reveals how scale structure, rhizome morphology, presence/absence of hydathodes and/or phyllopodia, and general growth form are important synapomorphies for sectional and subsectional classification in Elaphoglossum. The first major clade is formed by species with subulate scales and/or hydathodes. Within this clade, a monophyletic group is formed by those species possessing hydathodes, and another monophyletic group is formed by species lacking hydathodes. The second major clade is formed by species that generally have conspicuously scaly blades. The third major clade is characterized by slender, long-creeping, two-ranked rhizomes, small leaves ( generally less than 20 cm long), and echinulate spores. The fourth clade has phyllopodia and inconspicuously scaly or glabrous blades but is separated in two subgroups, one consisting of small plants with short-to long-creeping rhizomes and another of relatively larger plants with thicker, more congested rhizomes. The fifth clade consists solely of Elaphoglossum amygdalifolium, which differs from all other members of the genus by the combination of long-creeping rhizomes, hydathodes, phyllopodia, and reddish young leaves. Hydathodes have evolved independently more than once in Elaphoglossum. C1 Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20560 USA. New York Bot Garden, Bronx, NY 10458 USA. George Mason Univ, Dept Environm Sci & Policy 5FZ, Fairfax, VA 22030 USA. RP Skog, JE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20560 USA. EM jskog@gmu.edu RI Zimmer, Elizabeth/G-3890-2011 NR 35 TC 52 Z9 60 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD NOV PY 2004 VL 165 IS 6 BP 1063 EP 1075 DI 10.1086/423877 PG 13 WC Plant Sciences SC Plant Sciences GA 886RI UT WOS:000226245600015 ER PT J AU Gingerich, O AF Gingerich, O TI Catalogue of orbs, spheres and globes. 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, 60 Garden St, 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 NOV PY 2004 VL 35 BP 489 EP 490 PN 4 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 872KX UT WOS:000225207200011 ER PT J AU Kornicker, LS AF Kornicker, LS TI Morphology of the sixth limb of the Cypridinidae (Ostracoda : Myodocopina) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB Based on a comparison of the internal musculature of the fifth and sixth limbs of the cypridinid ostracode Isocypridina quatuorsetae, it is tentatively concluded that the sixth limbs of members of the Cypridinidae are biramous, each bearing an exopod represented by a cluster of small bristles (setae) and an endopod with two podomeres. The protopod contains a coxa with two endites and a basis with one endite. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20013 USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20013 USA. EM Kornicker.louis@nmnh.si.edu NR 17 TC 1 Z9 1 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 2004 VL 24 IS 4 BP 537 EP 540 DI 10.1651/C-2498 PG 4 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 877MW UT WOS:000225575700003 ER PT J AU Kim, TW Christy, JH Choe, JC AF Kim, TW Christy, JH Choe, JC TI Semidome building as sexual signaling in the fiddler crab Uca lactea (Brachyura : Ocypodidae) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID SEMILUNAR COURTSHIP RHYTHM; SENSORY TRAP HYPOTHESIS; PILLAR FUNCTION; ATTRACTIVENESS; CRUSTACEA; MUSICA; BEEBEI; TERPSICHORES; HOODS AB During the mating season, males of the fiddler crab Uca lactea build semidomes of mud at the entrances of their burrows to which they attract females for mating in the upper intertidal zone. Related species build similar structures which either reduce aggression between neighboring males or attract sexually receptive females. Male U. lactea did not build disproportionately more semidomes as density increased, suggesting that these structures do not modulate aggression. Larger males built higher and wider semidomes as would be expected if the semidomes are a courtship signal. When the high tides were too low to cover their habitat and the sediment dried, males were unable to build new or repair existing semidomes. Towards the end of the mating season more small males built semidomes perhaps because large males prevented them from courting earlier when most females mated. We made two experimental enclosures, added males to one and males and females to the other, and monitored semidome building. Males built significantly more semidomes in the enclosure with females. Overall, our observations support the hypothesis that the semidomes of U. lactea are a sexual signal. C1 Seoul Natl Univ, Sch Biol Sci, Lab Behav & Ecol, Seoul 151742, South Korea. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Choe, JC (reprint author), Seoul Natl Univ, Sch Biol Sci, Lab Behav & Ecol, Seoul 151742, South Korea. EM ocean74@snu.ac.kr; christyj@naos.si.edu; jcchoe@snu.ac.kr NR 23 TC 16 Z9 17 U1 1 U2 6 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 2004 VL 24 IS 4 BP 673 EP 679 DI 10.1651/C-2471 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 877MW UT WOS:000225575700015 ER PT J AU Bombardelli, C Lorenzini, EC Quadrelli, MB AF Bombardelli, C Lorenzini, EC Quadrelli, MB TI Retargeting dynamics of a linear tethered interferometer SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID SATELLITE AB The study deals with the issue of changing the plane of rotation (retargeting) of a linear kilometer-sized formation of two collectors and one combiner spacecraft connected by two tether arms. A control strategy is proposed that makes use of a pair of electrical thrusters located onboard two of the three spacecraft to redirect the angular momentum of the formation to a new target with an accuracy of a few arcseconds while keeping the angular momentum magnitude constant throughout the maneuver. The thruster profile is optimized to achieve a very smooth but relatively fast maneuver while maintaining the overall fuel consumption at a minimum level. The attitude dynamics of the formation are solved analytically based on a perturbation method, which allows calibrating the thrust profile for high-precision retargeting. A numerical model is employed to test the proposed strategy and to evaluate the influence of massive flexible tethers and external perturbations on the accuracy of the maneuver. Finally, the required propellant mass is evaluated with reference to envisioned space interferometry missions. C1 Univ Padua, Fac Engn, Ctr Interdipartimentale Studi & Attivita Spaziali, I-35131 Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bombardelli, C (reprint author), Univ Padua, Fac Engn, Ctr Interdipartimentale Studi & Attivita Spaziali, I-35131 Padua, Italy. NR 10 TC 16 Z9 17 U1 1 U2 5 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV-DEC PY 2004 VL 27 IS 6 BP 1061 EP 1067 DI 10.2514/1.2933 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 871QP UT WOS:000225148700015 ER PT J AU Dalebout, ML Baker, CS Mead, JG Cockcroft, VG Yamada, TK AF Dalebout, ML Baker, CS Mead, JG Cockcroft, VG Yamada, TK TI A comprehensive and validated molecular taxonomy of beaked whales, family Ziphiidae SO JOURNAL OF HEREDITY LA English DT Article ID MITOCHONDRIAL-DNA VARIATION; POPULATION-STRUCTURE; HUMPBACK WHALES; GENETIC IDENTIFICATION; INDOPACETUS-PACIFICUS; SEQUENCE DIVERGENCE; BALEEN WHALES; NUCLEAR; MESOPLODON; DIVERSITY AB DNA sequences from orthologous loci can provide universal characters for taxonomic identification. Molecular taxonomy is of particular value for groups in which distinctive morphological features are difficult to observe or compare. To assist in species identification for the little known family Ziphiidae (beaked whales), we compiled a reference database of mitochondrial DNA (mtDNA) control region (437 bp) and cytochrome b (384 bp) sequences for all 21 described species in this group. This mtDNA database is complemented by a nuclear database of actin intron sequences (925 bp) for 17 of the 21 species. All reference sequences were derived from specimens validated by diagnostic skeletal material or other documentation, and included four holotypes. Phylogenetic analyses of mtDNA sequences confirmed the genetic distinctiveness of all beaked whale species currently recognized. Both mitochondrial loci were well suited for species identification, with reference sequences for all known ziphiids forming robust species-specific clades in phylogenetic reconstructions. The majority of species were also distinguished by nuclear alleles. Phylogenetic comparison of sequence data from "test" specimens to these reference databases resulted in three major taxonomic discoveries involving animals previously misclassified from morphology. Based on our experience with this family and the order Cetacea as a whole, we suggest that a molecular taxonomy should consider the following components: comprehensiveness, validation, locus sensitivity, genetic distinctiveness and exclusivity, concordance, and universal accessibility and curation. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Ctr Dolphin Studies, ZA-6600 Plettenberg Bay, South Africa. Museum Nat Sci, Shinjuku Ku, Tokyo 1690073, Japan. Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. RP Baker, CS (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. EM cs.baker@auckland.ac.nz NR 90 TC 53 Z9 62 U1 0 U2 15 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 J9 J HERED JI J. Hered. PD NOV PY 2004 VL 95 IS 6 BP 459 EP 473 DI 10.1093/jhered/esh054 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 862HV UT WOS:000224482500001 PM 15475391 ER PT J AU Fritz, GN Engman, S Rodriguez, R Wilkerson, RC AF Fritz, GN Engman, S Rodriguez, R Wilkerson, RC TI Identification of four vectors of human Plasmodium spp. by multiplex PCR: Anopheles rangeli, An-strodei, An-triannulatus, and An-trinkae (Diptera : Culicidae : Nyssorhynchus) SO JOURNAL OF MEDICAL ENTOMOLOGY LA English DT Article DE An. rangeli; An. strodei; An. triannulatus; An. trinkae; polymerase chain reaction ID INTERNAL TRANSCRIBED SPACER; SPECIES DIAGNOSTIC ASSAY; RIBOSOMAL DNA; NUNEZTOVARI DIPTERA; SEQUENCE-ANALYSIS; GAMBIAE COMPLEX; MALARIA; HERMSI; FALCIPARUM; FREEBORNI AB One of the major obstacles for studies of the biology, ecology, and behavior of Neotropical vectors of human Plasmodiurn has been the lack of reliable and efficient means of identifying many species. Although the subgenus Nyssorhynchus includes most species responsible for human transmission in South America, there are no polymerase chain reaction (PCR) -based techniques for identifying members of this taxon. We describe the first multiplex PCR for identifying four species in the subgenus Nyssorhynchus that are vectors of human Plasmodium spp. Four species specific primers, together with a universal primer that anneals to the 5.8S rDNA region, produce amplicons of the internal transcribed spacer two with base pair sizes of 131, 308, 371, and 441 for An. triannulatus, An. trinkae, An. strodei, and An. rangeli, respectively. C1 Eastern Illinois Univ, Dept Biol Sci, Charleston, IL 61920 USA. Loyola Univ, Chicago Med Ctr, Cardiovasc Inst, Chicago, IL 60626 USA. Minist Salud & Previs Social, Escuela Tecn Salud Boliviano Japonesa, Cochabamba, Bolivia. Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Washington, DC 20013 USA. RP Fritz, GN (reprint author), Eastern Illinois Univ, Dept Biol Sci, Charleston, IL 61920 USA. FU NIAID NIH HHS [AI-31034] NR 33 TC 15 Z9 15 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0022-2585 J9 J MED ENTOMOL JI J. Med. Entomol. PD NOV PY 2004 VL 41 IS 6 BP 1111 EP 1115 DI 10.1603/0022-2585-41.6.1111 PG 5 WC Entomology; Veterinary Sciences SC Entomology; Veterinary Sciences GA 873JB UT WOS:000225274700015 PM 15605651 ER PT J AU Shin, J Lee, HS Kim, JY Shin, HJ Ahn, JW Paul, VJ AF Shin, J Lee, HS Kim, JY Shin, HJ Ahn, JW Paul, VJ TI New macrolides from the sponge Chondrosia corticata SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID NUDIBRANCH HEXABRANCHUS-SANGUINEUS; MARINE SPONGE; CYTOTOXIC MACROLIDES; MYCALE-MAGELLANICA; METABOLITES; MYCALOLIDES; HALICHONDRIA; ULAPUALIDE; EGGMASSES; OXAZOLE AB Three new oxazole-containing metabolites, neohalichondramide (5), (19Z)-halichondramide (6), and secohalichondramide (7), along with four previously reported compounds of the same structural class were isolated from the marine sponge Chondrosia corticata collected from Guam. The structures of novel compounds were determined on the basis of combined spectroscopic analyses. These compounds exhibited significant cytotoxicity and antifungal activity toward the human leukemia cell-line K562 and Candida albicans, respectively. C1 Seoul Natl Univ, Coll Pharm, Nat Prod Res Inst, Seoul 110460, South Korea. Korean Ocean Res & Dev Inst, Marine Nat Prod Lab, Seoul 425600, South Korea. Korea Maritime Univ, Div Ocean Sci, Pusan 606791, South Korea. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Shin, J (reprint author), Seoul Natl Univ, Coll Pharm, Nat Prod Res Inst, 28 Yungun, Seoul 110460, South Korea. EM shinj@snu.ac.kr; paul@sms.si.edu FU NIGMS NIH HHS [GM44796] NR 18 TC 15 Z9 17 U1 0 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD NOV PY 2004 VL 67 IS 11 BP 1889 EP 1892 DI 10.1021/np040124f PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 875TW UT WOS:000225445700023 PM 15568783 ER PT J AU Aguilera, O de Aguilera, DR AF Aguilera, O de Aguilera, DR TI Goliath grouper (Pisces : Serranidae) from the Upper Miocene Urumaco Formation, Venezuela SO JOURNAL OF PALEONTOLOGY LA English DT Article ID COLOMBIA; NEOGENE; FISHES C1 Univ Nacl Expt Francisco Miranda, Ctr Invest Ciencias Basicas, Complejo Docente Los Perozos, Coro 4101, Estado Falcon, Venezuela. Smithsonian Trop Res Inst, Panama City, Panama. RP Aguilera, O (reprint author), Univ Nacl Expt Francisco Miranda, Ctr Invest Ciencias Basicas, Complejo Docente Los Perozos, Carretera Variante Sur, Coro 4101, Estado Falcon, Venezuela. EM aguilero@unefm.edu.ve NR 26 TC 4 Z9 6 U1 3 U2 4 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 NOV PY 2004 VL 78 IS 6 BP 1202 EP 1206 DI 10.1666/0022-3360(2004)078<1202:GGPSFT>2.0.CO;2 PG 5 WC Paleontology SC Paleontology GA 866OC UT WOS:000224781800018 ER PT J AU Iati, MA Saija, R Giusto, A Denti, P Borghese, F Cecchi-Pestellini, C AF Iati, MA Saija, R Giusto, A Denti, P Borghese, F Cecchi-Pestellini, C TI Optical properties of interstellar grain aggregates SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE interstellar medium; grain aggregates; transition matrix; optical properties; radiation pressure ID 2 ELASTIC SPHERES; ULTRAVIOLET EXTINCTION; WAVELENGTH DEPENDENCE; DUST COAGULATION; ADHESIVE CONTACT; SCATTERING; RESISTANCE; PARTICLES; GRAPHITE; CLOUDS AB We computed, through the transition matrix method, the optical properties of cosmic dust grains modelled as aggregates (clusters) of spheres with a Gaussian-like size distribution function. The calculation is performed without resorting to any approximation and with a computational effort that is noticeably lighter than the one required by other methods. Our results show that particle clustering produces an enhancement in the extinction and radiation pressure cross-sections per unit mass. These results might help in the identification of sustainable structures for dust grains in the typical physical and chemical conditions of the diffuse interstellar medium. (C) 2004 Elsevier Ltd. All rights reserved. C1 Univ Messina, Dipartimento Fis Mat & Tecnol Fis Avanzate, I-98166 Messina, Italy. Ist Nazl Fis Mat, Unita Messina, I-98166 Messina, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. RP Borghese, F (reprint author), Univ Messina, Dipartimento Fis Mat & Tecnol Fis Avanzate, Salita Sperone 31, I-98166 Messina, Italy. EM borghese@ortica.unime.it OI Cecchi Pestellini, Cesare/0000-0001-7480-0324; IATI', MARIA ANTONIA/0000-0002-3576-8656; IATI', MARIA ANTONIA/0000-0003-0467-8049 NR 24 TC 4 Z9 4 U1 0 U2 0 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 NOV-DEC PY 2004 VL 89 IS 1-4 BP 43 EP 51 DI 10.1016/j.jqsrt.2004.05.010 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 856HP UT WOS:000224036600006 ER PT J AU Van Bael, SA Aiello, A Valderrama, A Medianero, E Samaniego, M Wright, SJ AF Van Bael, SA Aiello, A Valderrama, A Medianero, E Samaniego, M Wright, SJ TI General herbivore outbreak following an El Nino-related drought in a lowland Panamanian forest SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE canopy; defoliation; drought; El Nino Southern Oscillation; herbivory; Lepidoptera; outbreak; Panama; seasonally dry tropical forest ID TROPICAL TREE; DEFOLIATION; CANOPY; ABUNDANCE; PLANT; FOOD AB A severe outbreak of Lepidoptera followed the 1997-98 El Nino Southern Oscillation event, during which the climate in central Panama was unusually dry. The outbreak involved the larvae of at least 12 species of Lepidoptera and occurred at a seasonally dry, deciduous forest site, where extensive background data were available regarding climate, tree species and non-outbreak herbivory levels. Most Lepidoptera were associated with only one or two larval host plant species belonging to the same family, and the majority were monophagous during this study. During the outbreak, caterpillar densities for the major outbreak species averaged 1.6 larvae per young leaf and 0.18 larvae per leaf for leaves of all ages. For canopy trees and lianas, the mean level of leaf damage was 13.8%, ranging from 1-100%. Seven out of 20 tree species sustained most of the damage, with 21-37% of the leaf area consumed. Relative to non-outbreak years, damage levels increased by more than 250% during the outbreak. Single-species outbreaks were observed in other areas with a similar drought, but wetter forests in central Panama did not experience outbreaks during this period. Historically, fewer outbreaks have been reported from tropical forests than from temperate forests, however, similar El Nino-related outbreaks have occurred recently in several other locations throughout the tropics. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 30 TC 47 Z9 48 U1 1 U2 16 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 NOV PY 2004 VL 20 BP 625 EP 633 DI 10.1017/S0266467404001725 PN 6 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 876UU UT WOS:000225524400003 ER PT J AU Zotz, G AF Zotz, G TI The resorption of phosphorus is greater than that of nitrogen in senescing leaves of vascular epiphytes from lowland Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Barro Colorado Island; lowland forest; nutrient relations; resorption efficiency; resorption proficiency; senescence ID NUTRIENT RESORPTION; RAIN-FOREST; CARBON; BROMELIACEAE; CONSERVATION; LIMITATION; PATTERNS; LITTER C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 22 TC 23 Z9 24 U1 0 U2 15 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 NOV PY 2004 VL 20 BP 693 EP 696 DI 10.1017/S0266467404001889 PN 6 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 876UU UT WOS:000225524400009 ER PT J AU Wise, J Harasewych, MG Dillon, RT AF Wise, J Harasewych, MG Dillon, RT TI Population divergence in the sinistral whelks of North America, with special reference to the east Florida ecotone SO MARINE BIOLOGY LA English DT Article ID STARCH-GEL ELECTROPHORESIS; OYSTER CRASSOSTREA-VIRGINICA; MERCENARIA-MERCENARIA; GENE-SEQUENCES; DNA-SEQUENCES; PHYLOGENETIC ANALYSIS; SHELL MORPHOLOGY; HYBRID ZONE; HARD CLAM; MITOCHONDRIAL AB This study evaluated models of species relationships among sinistral whelks in the genus Busycon in the Atlantic and Gulf of Mexico. Gene frequencies at eight polymorphic allozyme loci, shell morphology, anatomy, and partial DNA sequences for the cytochrome c oxidase I (COI) mitochondrial gene were examined in eight populations, ranging from New Jersey to the Yucatan peninsula, and from the dextrally coiled sister taxon Busycon carica ( Gmelin, 1791). Whelks were collected in 1997 and 1998. The maximum COI sequence divergence recorded among 32 sinistral individuals was 1.96%, which together with the absence of any gross or qualitative morphological differences, suggested all eight populations should be considered conspecific. High levels of divergence between the allopatric western Atlantic and Gulf of Mexico populations, as revealed by fixed or nearly fixed differences at several allozyme-encoding loci were interpreted as evidence that the east Florida ecotone constitutes a significant barrier to gene flow. Size trimming also revealed several significant quantitative differences in shell and radular morphology between the three pooled Atlantic populations and five pooled Gulf populations. The Yucatan sample was the most distinctive conchologically, with heavy spines and tumid ridges, possibly related to stone crab predation. Based on the evidence all left-handed whelks of North America should be referred to the oldest available nomen, Busycon perversum (Linne, 1758), with three subspecies, B. perversum perversum along the Yucatan peninsula, B. perversum sinistrum (Hollister, 1958) in the northern and eastern Gulf of Mexico, and B. perversum laeostomum ( Kent, 1982) in the Atlantic. C1 Houston Museum Nat Sci, Houston, TX 77030 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA. Coll Charleston, Dept Biol, Charleston, SC 29424 USA. RP Wise, J (reprint author), Houston Museum Nat Sci, 1 Hermann Circle Dr, Houston, TX 77030 USA. EM jwise@hmns.org NR 64 TC 17 Z9 19 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD NOV PY 2004 VL 145 IS 6 BP 1167 EP 1179 DI 10.1007/s00227-004-1411-x PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 868BT UT WOS:000224888100010 ER PT J AU Duran, S Palacin, C Becerro, MA Turon, X Giribet, G AF Duran, S Palacin, C Becerro, MA Turon, X Giribet, G TI Genetic diversity and population structure of the commercially harvested sea urchin Paracentrotus lividus (Echinodermata, Echinoidea) SO MOLECULAR ECOLOGY LA English DT Article DE Atlanto-Mediterranean distribution; cytochrome c oxidase subunit I; mtDNA; Paracentrotus lividus; population genetic structure; sea urchin ID 2 CONTRASTING HABITATS; MITOCHONDRIAL-DNA; SPATIAL VARIABILITY; ALGAL ASSEMBLAGES; MEDITERRANEAN SEA; ATLANTIC; DISPERSAL; PHYLOGEOGRAPHY; PATTERNS; GROWTH AB The population structure of the edible Atlanto-Mediterranean sea urchin Paracentrotus lividus is described by analysing sequence variation in a fragment of the mitochondrial gene cytochrome c oxidase subunit I in 127 individuals from 12 localities across south-west Europe. The study revealed high levels of genetic diversity but low levels of genetic structure, suggesting a large degree of gene flow between populations and panmixis within each, the Mediterranean and Atlantic basins. However, we found significant genetic differentiation between the two basins probably due to restricted gene flow across the geographical boundary imposed by the area of the Strait of Gibraltar. Populations of P. lividus appeared to have experienced a recent demographic expansion in the late Pleistocene. We provide new evidence on the population structure of this commercial species, predicting a healthy stock of this sea urchin on the Mediterranean and Atlantic coasts. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Univ Barcelona, Dept Anim Biol Invertebrates, E-08028 Barcelona, Spain. CSIC, CEAB, Ctr Adv Studies, E-17300 Girona, Spain. Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. RP Duran, S (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM duran@sms.si.edu RI Becerro, Mikel/A-5325-2008; Turon, Xavier/J-9211-2012; Giribet, Gonzalo/P-1086-2015; OI Turon, Xavier/0000-0002-9229-5541; Giribet, Gonzalo/0000-0002-5467-8429; Becerro, Mikel/0000-0002-6047-350X NR 82 TC 79 Z9 83 U1 1 U2 16 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2004 VL 13 IS 11 BP 3317 EP 3328 DI 10.1111/j.1365-294X.2004.02338.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 862XF UT WOS:000224524000006 PM 15487992 ER PT J AU Yahr, R Vilgalys, R Depriest, PT AF Yahr, R Vilgalys, R Depriest, PT TI Strong fungal specificity and selectivity for algal symbionts in Florida scrub Cladonia lichens SO MOLECULAR ECOLOGY LA English DT Article DE Cladonia; Florida scrub; photobiont; selectivity; specificity; symbiosis ID NOSTOC-CONTAINING LICHENS; HOST-SPECIFICITY; TELL US; PHOTOBIONT; COMMUNITY; EVOLUTION; SPECIALIZATION; COEVOLUTION; DIVERSITY; PHYLOGENY AB Symbiosis is a major theme in the history of life and can be an important force driving evolution. However, across symbioses, it is difficult to tease apart the mechanisms that structure the interactions among potential partners. We used genetic similarity and frequency-based methods to qualitatively and quantitatively examine the patterns of association among several co-occurring Cladonia lichen fungi and their algal photobionts in six disjunct Florida scrub sites. The patterns of association were described by the degree of specificity, i.e. the phylogenetic range of associated partners, and of selectivity, i.e. the frequency of association among partners. Six fungal species associated with only one algal internal transcribed spacer clade, with the remaining two fungi being associated with two algal clades. In all cases, the fungi associated in unequal frequencies with the observed algal photobiont genotypes within those clades - suggesting that both specificity and selectivity were higher than expected. Fungal species can be grouped into three significantly different specificity classes: photobiont specialists, intermediates and generalists. In contrast to the pronounced specificity for photobionts among fungal species, the different Florida scrub sites do not harbour distinct photobiont pools, and differential photobiont availability cannot explain the patterning of lichen associations at this spatial scale. Therefore, we conclude that fungal specificity and selectivity for algal photobionts are major factors in determining the local composition of symbiotic partnerships. C1 Duke Univ, Dept Biol, Durham, NC 27708 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. RP Yahr, R (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. EM ry2@duke.edu RI DePriest, Paula/K-6633-2015; OI Vilgalys, Rytas/0000-0001-8299-3605 NR 48 TC 67 Z9 69 U1 3 U2 19 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2004 VL 13 IS 11 BP 3367 EP 3378 DI 10.1111/j.1365-294X.2004.02350.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 862XF UT WOS:000224524000010 PM 15487996 ER PT J AU Lidgard, DC Boness, DJ Bowen, WD McMillan, JI Fleischer, RC AF Lidgard, DC Boness, DJ Bowen, WD McMillan, JI Fleischer, RC TI The rate of fertilization in male mating tactics of the polygynous grey seal SO MOLECULAR ECOLOGY LA English DT Article DE alternative mating tactics; microsatellites; paternity; pinnipeds; reproductive behaviour ID HALICHOERUS-GRYPUS; PHOCA-VITULINA; SABLE ISLAND; NOVA-SCOTIA; PATERNITY; SUCCESS; POPULATIONS; BEHAVIOR; MARKERS AB Studies using molecular markers have shown that some grey seal males may be gaining success through exhibiting alternative mating tactics. We estimated the probability of fertilization success of grey seal males exhibiting the primary tactic of female defence and one alternative tactic of mating with departing females on Sable Island, Nova Scotia, Canada, during the breeding seasons of 1997-2002. Although the fertilization rate of the primary tactic (27-43%) was greater than that of the alternative tactic (10-12%), these low rates indicate the potential fitness value of alternative mating tactics in this size-dimorphic pinniped species. C1 Univ La Rochelle, Lab Biol & Environm Marins, F-17000 La Rochelle, France. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA. Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, Dartmouth, NS B2Y 4A2, Canada. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, Washington, DC 20008 USA. RP Univ St Andrews, Gatty Marine Lab, Sea Mammal Res Unit, St Andrews KY16 8LB, Fife, Scotland. EM dcl2@st-andrews.ac.uk RI Bowen, William/D-2758-2012 NR 22 TC 19 Z9 19 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2004 VL 13 IS 11 BP 3543 EP 3548 DI 10.1111/j.1365-294X.2004.02334.x PG 6 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 862XF UT WOS:000224524000024 PM 15488010 ER PT J AU Jonker, PG Galloway, DK McClintock, JE Buxton, M Garcia, M Murray, S AF Jonker, PG Galloway, DK McClintock, JE Buxton, M Garcia, M Murray, S TI Optical and X-ray observations of the neutron star soft X-ray transient XTE J1709-267 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : general; stars : individual : XTE J1709-267; stars : individual : 4U 1636-53; stars : neutron; X-rays : binaries ID BLACK-HOLE CANDIDATE; GLOBULAR-CLUSTERS; CENTAURUS X-4; AQUILA X-1; CHANDRA OBSERVATIONS; ROSAT OBSERVATIONS; ASCA OBSERVATIONS; THERMAL EMISSION; RADIO PULSARS; XMM-NEWTON AB In this paper we report on the discovery of the optical counterpart to the neutron star soft X-ray transient (SXT) XTE J1709-267 at an R-band magnitude of R=20.5+/-0.1 and 22.24+/-0.03, in outburst and quiescence, respectively. We further report the detection of type I X-ray bursts in RXTE data obtained during an outburst of the source in 2002. These bursts show a precursor before the onset of the main burst event, reminiscent of photospheric radius expansion bursts. Sifting through the archival RXTE data for the burster 4U 1636-53, we found a nearly identical burst with precursor in 4U 1636-53. A comparison of this burst to true photospheric radius expansion bursts in 4U 1636-53 leads us to conclude that these bursts-with-precursor do not reach the Eddington limit. Nevertheless, from the burst properties we can derive that the distance to XTE J1709-267 is consistent with the distance of the Globular Cluster NGC 6293. We further report on the analysis of a 22.7 ks observation of XTE J1709-267 obtained with the Chandra satellite when the source was in quiescence. We found that the source has a soft quiescent spectrum which can be fit well by an absorbed black body or neutron star atmosphere model. A power law contributes less than similar to20 per cent to the 0.5-10 keV unabsorbed flux of (1.0+/-0.3)x10(13) erg cm(-2) s(-1). This flux is only slightly lower than the flux measured right after the outburst in 2002. This is in contrast to the recent findings for MXB 1659-29, where the quiescent source flux decreased gradually by a factor of similar to7-9 over a period of 18 months. Finally, we compared the fractional power-law contribution to the unabsorbed 0.5-10 keV luminosity for neutron star SXTs in quiescence for which the distance is well-known. We find that the power-law contribution is low only when the source quiescent luminosity is close to similar to1-2x10(33) erg s(-1). Both at higher and lower values the power-law contribution to the 0.5-10 keV luminosity increases. We discuss how models for the quiescent X-ray emission can explain these trends. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pjonker@cfa.harvard.edu OI Galloway, Duncan/0000-0002-6558-5121 NR 73 TC 60 Z9 60 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 NOV 1 PY 2004 VL 354 IS 3 BP 666 EP 674 DI 10.1111/j.1365-2966.2004.08246.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864KX UT WOS:000224633500004 ER PT J AU Furlanetto, SR Hernquist, L Zaldarriaga, M AF Furlanetto, SR Hernquist, L Zaldarriaga, M TI Constraining the topology of reionization through Ly alpha absorption SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : high-redshift; intergalactic medium; quasars : absorption lines; cosmology : theory ID GUNN-PETERSON TROUGH; MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; INTERGALACTIC MEDIUM; HIGH-REDSHIFT; STAR-FORMATION; GALAXY FORMATION; EMISSION-LINES; DARK-MATTER; UNIVERSE AB The reionization of hydrogen in the intergalactic medium (IGM) is a crucial landmark in the history of the Universe, but the processes through which it occurs remain mysterious. In particular, recent numerical and analytic work suggest that reionization by stellar sources is driven by large-scale density fluctuations and must be inhomogeneous on scales of many comoving Mpc. We examine the prospects for constraining the topology of neutral and ionized gas through Lyalpha absorption of high-redshift sources. One method is to search for gaps in the Gunn-Peterson absorption troughs of luminous sources. These could occur if the line of sight passes sufficiently close to the centre of a large H II region. In contrast to previous work, we find a non-negligible (though still small) probability of observing such a gap before reionization is complete. In our model the transmission spike at z=6.08 in the spectrum of SDSS J1148+5251 does not necessarily require overlap to have been completed at an earlier epoch. We also examine the IGM damping wing absorption of the Lyalpha emission lines of star-forming galaxies. Because most galaxies sit inside of large H II regions, we find that the severity of absorption is significantly smaller than previously thought and decoupled from the properties of the observed galaxy. While this limits our ability to constrain the mean neutral fraction of the IGM from observations of individual galaxies, it presents the exciting possibility of measuring the size distribution and evolution of the ionized bubbles by examining the distribution of damping wing optical depths in a large sample of galaxies. 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 Furlanetto, SR (reprint author), CALTECH, Div Phys Math & Astron, Mail Code 130-33, Pasadena, CA 91125 USA. EM sfurlane@tapir.caltech.edu NR 66 TC 61 Z9 61 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2004 VL 354 IS 3 BP 695 EP 707 DI 10.1111/j.1365-2966.2004.08225.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864KX UT WOS:000224633500007 ER PT J AU Reda, FM Forbes, DA Beasley, MA O'Sullivan, EJ Goudfrooij, P AF Reda, FM Forbes, DA Beasley, MA O'Sullivan, EJ Goudfrooij, P TI The photometric properties of isolated early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : elliptical and lenticular cD galaxies : luminosity function, mass function; galaxies : photometry; galaxies : structure ID COLOR-MAGNITUDE RELATION; CCD SURFACE PHOTOMETRY; X-RAY-PROPERTIES; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; FUNDAMENTAL PLANE; STATISTICAL PROPERTIES; INTERSTELLAR MATTER; KORMENDY RELATION; DISTANT CLUSTERS AB Isolated galaxies are important because they probe the lowest density regimes inhabited by galaxies. We define a sample of 36 nearby isolated early-type galaxies for further study. Our isolation criteria require them to have no comparable-mass neighbours within 2 B-band magnitudes, 0.67 Mpc in the plane of the sky and 700 km s(-1) in recession velocity. New widefield optical imaging of 10 isolated galaxies with the Anglo-Australian Telescope confirms their early-type morphology and relative isolation. We also present imaging of four galaxy groups as a control sample. The isolated galaxies are shown to be more gravitationally isolated than the group galaxies. We find that the isolated early-type galaxies have a mean effective colour of (B0R)(e) = 1.54 +/- 0.14, similar to their high-density counterparts. They reveal a similar colour-magnitude relation slope and small intrinsic scatter to cluster ellipticals. They also follow the Kormendy relation of surface brightness versus size for luminous cluster galaxies. Such properties suggest that the isolated galaxies formed at a similar epoch to cluster galaxies, such that the bulk of their stars are very old. However, our galaxy modelling reveals evidence for dust lanes, plumes, shells, boxy and disc isophotes in four out of nine galaxies. Thus at least some isolated galaxies have experienced a recent merger/accretion event, which may have induced a small burst of star formation. We derive luminosity functions for the isolated galaxies and find a faint slope of -1.2, which is similar to the 'universal' slope found in a wide variety of environments. We examine the number density distribution of galaxies in the field of the isolated galaxies. Only the very faintest dwarf galaxies (M-R greater than or similar to -15.5) appear to be associated with the isolated galaxies, whereas any intermediate-luminosity galaxies appear to lie in the background. Finally, we discuss possible formation scenarios for isolated early-type galaxies. Early epoch formation and a merger/accretion of galaxies are possible explanations. The collapse of a large, virialized group is an unlikely explanation, but that of a poor group remains viable. C1 Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Natl Res Inst Astron & Geophys, Dept Astron, Cairo 11421, Egypt. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Reda, FM (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM freda@astro.swin.edu.au; dforbes@swin.edu.au; mbeasley@ucolick.org; ejos@head-cfa.cfa.harvard.edu; goudfroo@stsci.edu OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 97 TC 63 Z9 63 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2004 VL 354 IS 3 BP 851 EP 869 DI 10.1111/j.1365-2966.2004.08250.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864KX UT WOS:000224633500024 ER PT J AU O'Sullivan, E Ponman, TJ AF O'Sullivan, E Ponman, TJ TI The isolated elliptical NGC 4555 observed with Chandra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : individual : NGC 4555; X-rays : galaxies ID EARLY-TYPE GALAXIES; MULTIPHASE HOT GAS; X-RAY CONSTRAINTS; DARK-MATTER; XMM-NEWTON; SPECTRAL PROPERTIES; NEARBY GROUPS; CLUSTERS; MASS; EVOLUTION AB We present analysis of a Chandra observation of the elliptical galaxy NGC 4555. The galaxy lies in a very low density environment, either isolated from all galaxies of similar mass or on the outskirts of a group. Despite this, NGC 4555 has a large gaseous halo, extending to similar to60 kpc. We find the mean gas temperature to be similar to0.95 keV and the Fe abundance to be similar to0.5 Z(.).We model the surface brightness, temperature and abundance distribution of the halo and use these results to estimate parameters such as the entropy and cooling time of the gas, and the total gravitational mass of the galaxy. In contrast to recent results showing that moderate luminosity ellipticals contain relatively small quantities of dark matter, our results show that NGC4555 has a massive dark halo and large mass-to-light ratio (56.8(-35.8)(+34 2) M-./ L-B. at 50 kpc, 42.7(-21.2)(+14 6) at 5r(e), 1sigma errors). We discuss this disparity and consider possible mechanisms by which galaxies might reduce their dark matter content. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ejos@head.cfa.harvard.edu OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 59 TC 36 Z9 36 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2004 VL 354 IS 3 BP 935 EP 944 DI 10.1111/j.1365-2966.2004.08257.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864KX UT WOS:000224633500032 ER PT J AU Yuan, F Zdziarski, AA AF Yuan, F Zdziarski, AA TI Luminous hot accretion flows: the origin of X-ray emission from Seyfert galaxies and black hole binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; hydrodynamics; radiation mechanisms : thermal; galaxies : active; galaxies : nuclei ID ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; OUTER BOUNDARY-CONDITION; NOVA MUSCAE 1991; CYGNUS X-1; THERMAL COMPTONIZATION; SPECTRAL TRANSITIONS; CENTRAL REGIONS; THIN CLOUDS; DISK MODELS AB We investigate accretion disc models for the X-ray emission of type 1 Seyfert galaxies and the hard state of black hole binaries. We concentrate on two hot accretion disc models: advection-dominated accretion flow( ADAF) and the recently found luminous hot accretion flow( LHAF). We solve for the global solution of both ADAF and LHAF to obtain the electron temperature, T-e, and Thomson optical depth, tau, at the radius where most of the radiation comes from. We adopt two kinds of electron energy equations. In one, only synchrotron and bremsstrahlung radiation and their Comptonization are considered. The other is parametrized by a constant Compton parameter to model the case in which thermal Comptonization of external soft photons is important. We compare the calculated T-e and with the observational values obtained by fitting the average spectra of type 1 Seyfert galaxies and black hole binaries using the thermal-Comptonization model. We find that the most favoured model is an LHAF with a parametrized electron energy equation, with ADAFs predicting a too-high T-e. Also, LHAF, but not ADAF, can explain the large luminosities in excess of 10 per cent of the Eddington luminosity seen in the hard state of transient black hole binaries. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Ctr Astron M Kopernika, PL-00716 Warsaw, Poland. RP Yuan, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fyuan@physics.purdue.edu; aaz@camk.edu.pl NR 78 TC 36 Z9 36 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2004 VL 354 IS 3 BP 953 EP 960 DI 10.1111/j.1365-2966.2004.08262.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 864KX UT WOS:000224633500034 ER PT J AU Keita, SOY Kittles, RA Royal, CDM Bonney, GE Furbert-Harris, P Dunston, GM Rotimi, CN AF Keita, SOY Kittles, RA Royal, CDM Bonney, GE Furbert-Harris, P Dunston, GM Rotimi, CN TI Conceptualizing human variation SO NATURE GENETICS LA English DT Article ID LINKAGE-DISEQUILIBRIUM; HUMAN-POPULATIONS; GENETIC DIVERSITY; ASSOCIATION; RACE; DISEASE; GENOME AB What is the relationship between the patterns of biological and sociocultural variation in extant humans? Is this relationship accurately described, or best explained, by the term 'race' and the schema of 'racial' classification? What is the relationship between 'race', genetics and the demographic groups of society? Can extant humans be categorized into units that can scientifically be called 'races'? These questions underlie the discussions that address the explanations for the observed differences in many domains between named demographic groups across societies. These domains include disease incidence and prevalence and other variables studied by biologists and social scientists. Here, we offer a perspective on understanding human variation by exploring the meaning and use of the term 'race' and its relationship to a range of data. The quest is for a more useful approach with which to understand human biological variation, one that may provide better research designs and inform public policy. C1 Howard Univ, Coll Med, Natl Human Genome Ctr, Washington, DC 20060 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. Ohio State Univ, Dept Mol Virol Immunol & Med Genet, Columbus, OH 43210 USA. RP Kittles, RA (reprint author), Howard Univ, Coll Med, Natl Human Genome Ctr, Washington, DC 20060 USA. EM kittles-1@medctr.osu.edu NR 36 TC 60 Z9 63 U1 0 U2 9 PU NATURE PUBLISHING GROUP PI NEW YORK PA 345 PARK AVE SOUTH, NEW YORK, NY 10010-1707 USA SN 1061-4036 J9 NAT GENET JI Nature Genet. PD NOV PY 2004 VL 36 IS 11 SU S BP S17 EP S20 DI 10.1038/ng1455 PG 4 WC Genetics & Heredity SC Genetics & Heredity GA 867PH UT WOS:000224854000006 PM 15507998 ER PT J AU Santamore, DH Goan, HS Milburn, GJ Roukes, ML AF Santamore, DH Goan, HS Milburn, GJ Roukes, ML TI Anharmonic effects on a phonon-number measurement of a quantum-mesoscopic-mechanical oscillator SO PHYSICAL REVIEW A LA English DT Article ID RESONATOR AB We generalize a proposal for detecting single-phonon transitions in a single nanoelectromechanical system (NEMS) to include the intrinsic anharmonicity of each mechanical oscillator. In this scheme two NEMS oscillators are coupled via a term quadratic in the amplitude of oscillation for each oscillator. One NEMS oscillator is driven and strongly damped and becomes a transducer for phonon number in the other measured oscillator. We derive the conditions for this measurement scheme to be quantum limited and find a condition on the size of the anharmonicity. We also derive the relation between the phase diffusion back-action noise due to number measurement and the localization time for the measured system to enter a phonon-number eigenstate. We relate both these time scales to the strength of the measured signal, which is an induced current proportional to the position of the read-out oscillator. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. CALTECH, Dept Phys, Pasadena, CA 91125 USA. Univ New S Wales, Ctr Quantum Comp Technol, Sydney, NSW 2052, Australia. Univ Queensland, Ctr Quantum Comp Technol, St Lucia, Qld 4072, Australia. RP Santamore, DH (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RI MIlburn, Gerard/B-6381-2008; Roukes, Michael/E-9787-2010 OI MIlburn, Gerard/0000-0002-5404-9681; NR 19 TC 23 Z9 23 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2004 VL 70 IS 5 AR 052105 DI 10.1103/PhysRevA.70.052105 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 876EM UT WOS:000225479000019 ER PT J AU Wang, T Kostrun, M Yelin, SF AF Wang, T Kostrun, M Yelin, SF TI Multiple beam splitter for single photons SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; RAMAN ADIABATIC PASSAGE; ATOMIC ENSEMBLES; QUANTUM COMMUNICATION; ENTANGLEMENT; STATES; LIGHT; COHERENCE; CREATION; STORAGE AB We propose a method using "light storage" and fractional stimulated Raman adiabatic passage (F-STIRAP) to get entangled multiple Fock states from a single photon. A light storage technique is used to store the quantum information of a single-photon pulse in atoms. F-STIRAP pulses then split the stored coherence, such that reading pulses retrieve the quantum information from this new coherence. Since each reading pulse only retrieves part of the total coherence, we can obtain entangled multiple Fock states with arbitrary relative amplitude. This method to create entanglement is versatile for obtaining frequency, time, and/or spatial entanglement. Indeed, we obtain a multiple beam splitter with easily adjustable parameters. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. NR 32 TC 27 Z9 27 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 2004 VL 70 IS 5 AR 053822 DI 10.1103/PhysRevA.70.053822 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 876EM UT WOS:000225479000148 ER PT J AU Kirby, K Houle, FA AF Kirby, K Houle, FA TI Ethics and the welfare of the physics profession SO PHYSICS TODAY LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. IBM Corp, Almaden Res Ctr, San Jose, CA USA. RP Kirby, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 9 Z9 9 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 0031-9228 J9 PHYS TODAY JI Phys. Today PD NOV PY 2004 VL 57 IS 11 BP 42 EP 46 DI 10.1063/1.1839376 PG 5 WC Physics, Multidisciplinary SC Physics GA 867WJ UT WOS:000224873100025 ER PT J AU Zotz, G Enslin, A Hartung, W Ziegler, H AF Zotz, G Enslin, A Hartung, W Ziegler, H TI Physiological and anatomical changes during the early ontogeny of the heteroblastic bromeliad, Vriesea sanguinolenta, do not concur with the morphological change from atmospheric to tank form SO PLANT CELL AND ENVIRONMENT LA English DT Article DE abscisic acid; heteroblasty; intraspecific variability; leaf nitrogen; ontogenetic drift; photosynthesis; phyllotaxis; specific leaf area; vascular epiphytes; water relations ID TILLANDSIA-DEPPEANA BROMELIACEAE; PLANT SIZE; ECOPHYSIOLOGICAL CONSEQUENCES; VASCULAR EPIPHYTES; ABSCISIC-ACID; JUVENILE; WATER; TOLERANCE AB Two distinct morphological forms characterize the ontogeny of many epiphytic bromeliads. Smaller plants exhibit an atmospheric habit, while larger plants form water-impounding tanks. The study of the functional significance of heteroblasty in epiphytes is severely hampered by considerable size-related variation in morphological, anatomical and physiological parameters. To overcome this problem, plants of varying size of both atmospheric and tank form were included in the present study with Vriesea sanguinolenta. The results show that virtually all morphological, anatomical and physiological characteristics vary during ontogeny, but changes were rarely directly related to the step change in gross morphology. Changes were either: (1) gradual from smallest atmospheric to small tank (e.g. leaf divergence angles, reduction in photosystem II efficiency during drought, speed of recovery after drought); (2) there was no change between atmospheric and small tank, but a gradual or step change within the tank form (stomatal density, relationship of leaf N and specific leaf area); or (3) developmental patterns were more complicated with decreases and increases during ontogeny (photosynthetic capacity, carbon isotope ratios, abscisic acid levels during drought). Although the comparisons between ontogenetic phases were always confounded by size differences, a hypothetical small tank plant is expected to suffer higher water loss than a real atmospheric, whereas a hypothetical, large atmospheric plant would show reduced access to resources, such as nutrients, in comparison with the real tank. The present results are consistent with the notion of heteroblasty as an adaptation of early ontogenetic stages to drought, but highlight that size-related variation greatly modifies any difference directly associated with the step change from atmospheric to tank. C1 Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. Smithsonian Trop Res Inst, Balboa, Panama. Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. Univ Wurzburg, Lehrstuhl Bot 1, D-8700 Wurzburg, Germany. Tech Univ Munich, Lehrstuhl Bot, D-85354 Freising Weihenstephan, Germany. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. EM gerhard.zotz@unibas.ch NR 38 TC 12 Z9 14 U1 0 U2 15 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD NOV PY 2004 VL 27 IS 11 BP 1341 EP 1350 DI 10.1111/j.1365-3040.2004.01223.x PG 10 WC Plant Sciences SC Plant Sciences GA 872DY UT WOS:000225188800002 ER PT J AU Verwichte, E Nakariakov, VM Ofman, L Deluca, EE AF Verwichte, E Nakariakov, VM Ofman, L Deluca, EE TI Characteristics of transverse oscillations in a coronal loop arcade SO SOLAR PHYSICS LA English DT Article ID MAGNETOHYDRODYNAMIC WAVES; NUMERICAL SIMULATIONS; RESONANT ABSORPTION; TRANSITION-REGION; TRACE; EXPLORER; FLARE; HOT AB TRACE observations from 15 April 2001 of transverse oscillations in coronal loops of a post-flare loop arcade are investigated. They are considered to be standing fast kink oscillations. Oscillation signatures such as displacement amplitude, period, phase and damping time are deduced from 9 loops as a function of distance along the loop length. Multiple oscillation modes are found with different amplitude profile along the loop length, suggesting the presence of a second harmonic. The damping times are consistent with the hypothesis of phase mixing and resonant absorption, although there is a clear bias towards longer damping times compared with previous studies. The coronal magnetic field strength and coronal shear viscosity in the loop arcade are derived. C1 Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Verwichte, E (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RI Nakariakov, Valery/E-2375-2013; Lee, SungHwan/O-2563-2013; DeLuca, Edward/L-7534-2013 OI Nakariakov, Valery/0000-0001-6423-8286; DeLuca, Edward/0000-0001-7416-2895 NR 30 TC 171 Z9 172 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2004 VL 223 IS 1 BP 77 EP 94 DI 10.1007/s11207-004-0807-6 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902EK UT WOS:000227336600006 ER PT J AU Schmieder, B Mein, N Deng, YY Dumitrache, C Malherbe, JM Staiger, J Deluca, EE AF Schmieder, B Mein, N Deng, YY Dumitrache, C Malherbe, JM Staiger, J Deluca, EE TI Magnetic changes observed in the formation of two filaments in a complex active region: Trace and MSDP observations SO SOLAR PHYSICS LA English DT Article ID CONFIGURATIONS SUPPORTING PROMINENCES; VARIABLE SOURCE FUNCTION; H-ALPHA STRUCTURES; C-IV LINES; TRANSITION REGION; CORONAL EXPLORER; FINE-STRUCTURE; LATERAL FEET; CLOUD MODEL; RECONNECTION AB This paper is focused on the formation of two filaments in a complex center of decaying active regions (AR 8329 and AR 8326), located in the northern hemisphere. The observations were obtained in Ha by the Multi-channel Subtractive Double Pass spectrograph (MSDP mounted on the German telescope VTT in Tenerife) and EUV lines with TRACE (Transition Region And Corona Explorer). High Doppler shifts are found to be related to the ends of filament segments where canceling magnetic fields are also located (as seen on magnetograms from Big Bear Solar Observatory). At these locations, velocities along the line of sight, derived by using a cloud model method reach -20 km s(-1), the segments of filaments merge and frequently a time-related sub-flare is observed by TRACE. The chirality of the filament segments has been determined by different methods: the segments of dextral chirality join together and form a long dextral filament, and a single filament of sinistral chirality forms end to end with the dextral filament but does not merge with it. Assuming a model of twisted flux tube for filament material, we suggest that the dextral filament has negative helicity and a relationship between its formation and the close by sunspot with the same sign of helicity. C1 Observ Paris, F-92195 Meudon, France. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Chinese Acad Sci, Beijing Astron Observ, Beijing 100012, Peoples R China. Acad Romana, Astron Inst, Bucharest 75212, Romania. Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA USA. RP Schmieder, B (reprint author), Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM brigitte.schmieder@obspm.fr; dyy@sun10.bao.ac.cn RI DeLuca, Edward/L-7534-2013; Dumitrache, Cristiana/B-8970-2011 OI DeLuca, Edward/0000-0001-7416-2895; Dumitrache, Cristiana/0000-0001-6059-4419 NR 32 TC 37 Z9 37 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD NOV PY 2004 VL 223 IS 1 BP 119 EP 141 DI 10.1007/s11207-004-1107-x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 902EK UT WOS:000227336600008 ER PT J AU Parenti, LR Humphries, CJ AF Parenti, LR Humphries, CJ TI Historical biogeography, the natural science SO TAXON LA English DT Article ID CLADISTIC BIOGEOGRAPHY; COMPONENT ANALYSIS; PHYLOGENY; DISPERSAL; AREAS C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Div Fishes, Washington, DC 20013 USA. Nat Hist Museum, Dept Bot, London SW7 5BD, England. RP Parenti, LR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Zool, Div Fishes, POB 37012,Rm WG-12,MRC 159, Washington, DC 20013 USA. EM parenti@si.edu; cjh@nhm.ac.uk NR 42 TC 11 Z9 11 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD NOV PY 2004 VL 53 IS 4 BP 899 EP 903 DI 10.2307/4135556 PG 5 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 887UY UT WOS:000226332200003 ER PT J AU Reveal, JL Gandhi, KN Nicolson, DH AF Reveal, JL Gandhi, KN Nicolson, DH TI The demise of the name Astragalus tenellus Pursh (Fabaceae) SO TAXON LA English DT Editorial Material DE Astragalus; Astragalus belangeri; Astragalus multiflorus; Astragalus tenellus; Ervum multiflorum; Fabaceae; nomenclature AB Rupert Barneby (1964) expressed "doubts of the legality" in adopting "Astragalus tenellus Pursh" (1813) over A. multiflorus (Pursh) A. Gray (1864). His concern was justified since Pursh invalidated his own name when he simultaneously published Ervum multiflorum (the basionym of A. multiflorus) on a different page in the same work and cited "A. tenellus" in synonymy. By the time Astragalus tenellus Pursh ex E. Sheld. (1894) was validly published, it was a later homonym as well as superfluous. Given the status of A. tenellus Bunge (1869), the name of an Old World species in current use, conservation of A. tenellus Pursh ex E. Sheld. is unlikely, and we recommend adoption of A. multiflorus for the North American plant. C1 New York Bot Gdn, Bronx, NY 10458 USA. Univ Maryland, College Pk, MD 20742 USA. Harvard Univ, Cambridge, MA 02138 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Reveal, JL (reprint author), 18625 Spring Canyon Rd, Montrose, CO 81401 USA. EM jr19@umail.umd.edu; kgandhi@oeb.harvard.edu; nicolson.dan@nmnh.si.edu NR 38 TC 0 Z9 0 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD NOV PY 2004 VL 53 IS 4 BP 1055 EP 1058 DI 10.2307/4135574 PG 4 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 887UY UT WOS:000226332200021 ER PT J AU Holtum, JAM Aranda, J Virgo, A Gehrig, HH Winter, K AF Holtum, JAM Aranda, J Virgo, A Gehrig, HH Winter, K TI delta(13)C values and crassulacean acid metabolism in Clusia species from Panama SO TREES-STRUCTURE AND FUNCTION LA English DT Article DE Clusia; crassulacean acid metabolism (CAM); photosynthetic pathway; stable carbon isotopes ID GENUS CLUSIA; GAS-EXCHANGE; MINOR L; VASCULAR EPIPHYTES; ISOTOPE RATIOS; CO2 FIXATION; WATER-STRESS; C3-CAM TREE; ROSEA JACQ; CAM AB The genus Clusia is notable in that it contains arborescent crassulacean acid metabolism (CAM) plants. As part of a study of CAM in Clusia, titratable acidities were measured in 25 species and delta(13)C values were measured for 38 species from Panama, including seven undescribed species, and 11 species from Colombia, Costa Rica and Honduras. CAM was detected in 12 species. Clusia flava, C. rosea and C. uvitana exhibited delta13C values or diurnal fluctuations in acidity indicative of strong CAM. In C. croatii, C. cylindrica, C. fructiangusta, C. lineata, C. odorata, C. pratensis, C. quadrangula, C. valerioi and C. sp. D diurnal fluctuations in acidity were consistent with weak CAM but the delta(13)C values were C(3)-like. All of the species that exhibited strong or weak CAM were in the C. flava or C. minor species groups. CAM was not detected in any member of the C. multiflora species group. Strong CAM species were not collected at altitudes above 680 m a.s.l. On the basis of delta(13)C values, the expression of CAM was similar in terrestrial, hemi-epiphytic and epiphytic species and did not differ between individuals of the same species that exhibited different life-forms. This study indicates that phylogenetic affiliation may be a predictor of an ability to exhibit CAM in Clusia species from the Panamanian region, and that weak CAM is probably a common photosynthetic option in many Clusia species. delta(13)C value is not a particularly good indicator of a potential of Clusia species growing in the field to exhibit CAM because it appears that the contribution in most species of CAM to carbon gain is generally rather small when integrated over the life-time of leaves. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. EM winterk@tivoli.si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 47 TC 41 Z9 43 U1 4 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0931-1890 J9 TREES-STRUCT FUNCT JI Trees-Struct. Funct. PD NOV PY 2004 VL 18 IS 6 BP 658 EP 668 DI 10.1007/s00468-004-0342-y PG 11 WC Forestry SC Forestry GA 866DZ UT WOS:000224755300006 ER PT J AU Cardini, A Ferraguti, M AF Cardini, A Ferraguti, M TI The phylogeny of Branchiobdellida (Annelida, Clitellata) assessed by sperm characters SO ZOOLOGISCHER ANZEIGER LA English DT Article DE spermatozoa; structure; branchiobdellidans; rates of evolution ID 18S RDNA; OLIGOCHAETA; SPERMATOZOA; HIRUDINEA; FAMILIES; LEECHES; ORIGIN AB Data on the spermatozoa of Branchiobdellida were taken from the published literature: sperm models of 25 species belonging to 13 different branchiobdellidan genera have been compared with the aim of supplying further evidences for a phylogenetic analysis of the group. The species considered were representative of all traditional branchiobdellidan families, excluding the monotypic Caridinophilidae. Branchiobdellidan spermatozoa are complex cells, thus it was possible to analyse the variation of 20 characters within the group. A parsimony analysis has yielded nine minimal trees, eight of which are very similar to one another. The main conclusions of the phylogenetic analysis are: (a) the monophyly of the taxon Branchiobdellida is confirmed; (b) the most speciose branchiobdellidan genus, Cambarincola is polyphyletic; (c) none of the traditional 'families' are supported; (d) the genus Branchiobdella is monophyletic, but the position of one species, B. kobayashi, albeit basal to the whole genus, is not resolved; (e) the other two genera analysed for which more than one species was available, Pterodrilus and Xironogiton, are monophyletic; (f) there seems to be a 'trend' in the whole group towards an increase of acrosome length. Our results partly parallel those obtained by Gelder and Siddall (2000) with a combined analysis of molecular and somatic characters, and point to the need for a comprehensive revision of the Branchiobdellida based on a combination of molecular, somatic and spermatological data sets. (C) 2004 Elsevier GmbH. All rights reserved. C1 Univ Milan, Ist Med Legale & Assicurazioni, Milan, Italy. Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Smithsonian Inst, Washington, DC 20560 USA. Univ Milan, Dipartimento Biol, Milan, Italy. RP Cardini, A (reprint author), Univ York, Hull York Med Sch, York YO10 5DD, N Yorkshire, England. EM alcardini@interfree.it; marco.ferraguti@unimi.it RI cardini, andrea/G-9951-2011 OI cardini, andrea/0000-0003-2910-632X NR 28 TC 15 Z9 15 U1 0 U2 2 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0044-5231 J9 ZOOL ANZ JI Zool. Anz. PD NOV PY 2004 VL 243 IS 1-2 BP 37 EP 46 DI 10.1016/j.jcz.2004.06.001 PG 10 WC Zoology SC Zoology GA 891TJ UT WOS:000226603600004 ER PT J AU Lachniet, MS Burns, SJ Piperno, DR Asmerom, Y Polyak, VJ Moy, CM Christenson, K AF Lachniet, MS Burns, SJ Piperno, DR Asmerom, Y Polyak, VJ Moy, CM Christenson, K TI A 1500-year El Nino/Southern Oscillation and rainfall history for the Isthmus of Panama from speleothem calcite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE paleoclimate; El Nino/Southern Oscillation; speleothem; Mdieval Climatic Anomaly; Intertropical Convergence Zone; Panama ID INTERTROPICAL CONVERGENCE ZONE; INTERANNUAL VARIABILITY; ISOTOPIC COMPOSITION; CARIBBEAN RAINFALL; TROPICAL ATLANTIC; MEDIEVAL TIME; PRECIPITATION; CLIMATE; CIRCULATION; STALAGMITE AB [1] The effect of the El Nino/Southern Oscillation (ENSO) on tropical rainfall variations of the past 2 millennia is largely unknown. High-resolution monsoon records are sparse, despite the role of ENSO in generating global hydrologic anomalies in modern climate. To investigate the relationship between ENSO and the Central American Monsoon, we generated a high-resolution ( similar to 2.9 years/sample) oxygen-isotope monsoon rainfall record from a U/Th-dated stalagmite ( 180 B. C. to 1310 A. D.) from the Isthmus of Panama. We present evidence for a weakened monsoon during the "High Medieval'' ( 1100 - 1200 A. D.) and the Classic Maya Collapse ( 750 - 950 A. D.). Rainfall decreased and was more variable after 550 A. D., and the period 900 - 1310 A. D. was drier than the preceding millennium. A weaker monsoon corresponds with increased El Nino variability, and our data display statistical variance in the ENSO band. We conclude that ENSO variation has forced isthmian rainfall and may have contributed to hemispheric climatic anomalies at this time. C1 Univ Nevada, Dept Geosci, Las Vegas, NV 89154 USA. Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. Stanford Univ, Dept Geog & Environm Sci, Stanford, CA 94305 USA. RP Univ Nevada, Dept Geosci, 4505 Maryland Pkwy,Box 4010, Las Vegas, NV 89154 USA. EM matthew.lachniet@ccmail.nevada.edu RI Burns, Stephen/H-9419-2013; OI Lachniet, Matthew/0000-0001-5250-0144 NR 35 TC 48 Z9 49 U1 1 U2 28 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 OCT 30 PY 2004 VL 109 IS D20 AR D20117 DI 10.1029/2004JD004694 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 867ZX UT WOS:000224882700002 ER PT J AU Pennington, RT Dick, CW AF Pennington, RT Dick, CW TI The role of immigrants in the assembly of the South American rainforest tree flora SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Discussion Meeting on Plant Phylogeny and the Origin of Major Biomes CY MAR 15-16, 2004 CL Royal Soc, London, ENGLAND HO Royal Soc DE Amazon rainforests; molecular systematics; biotic interchange; long-distance dispersal ID HISTORICAL BIOGEOGRAPHY; NORTHERN HEMISPHERE; DNA-SEQUENCES; PHYLOGENY; EVOLUTION; TERTIARY; CHLOROPLAST; VEGETATION; DIVERSITY; MIGRATION AB The Amazon lowland rainforest flora is conventionally viewed as comprising lineages that evolved in biogeographic isolation after the split of west Gondwana (ca. 100 Myr ago). Recent molecular phylogenies, however, identify immigrant lineages that arrived in South America during its period of oceanic isolation (ca. 100-3 Myr ago). Long-distance sweepstakes dispersal across oceans played an important and possibly predominant role. Stepping-stone migration from Africa and North America through hypothesized Late Cretaceous and Tertiary island chains may have facilitated immigration. An analysis of inventory plot data suggests that immigrant lineages comprise ca. 20% of both the species and individuals of an Amazon tree community in Ecuador. This is more than an order of magnitude higher than previous estimates. We also present data on the community-level similarity between South American and palaeo-tropical rainforests, and suggest that most taxonomic similarity derives from trans-oceanic dispersal, rather than a shared Gondwanan history. C1 Royal Bot Gardens, Edinburgh EH3 5LR, Midlothian, Scotland. Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. RP Pennington, RT (reprint author), Royal Bot Gardens, 20a Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland. EM t.pennington@rbge.org.uk RI Dick, Christopher/A-8744-2008 NR 29 TC 120 Z9 126 U1 3 U2 17 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD OCT 29 PY 2004 VL 359 IS 1450 BP 1611 EP 1622 DI 10.1098/rstb.2004.1532 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 868MW UT WOS:000224918700013 PM 15519976 ER PT J AU Betancur-R, R Acero, A AF Betancur-R, R Acero, A TI Description of Notarius biffi n. sp and redescription of N-insculptus (Jordan and Gilbert) (Siluriformes : Ariidae) from the eastern Pacific, with evidence of monophyly and limits of Notarius SO ZOOTAXA LA English DT Article DE Notarius biffi; Notarius insculptus; Ariidae; sea catfishes; eastern Pacific AB A new species of ariid catfish, Notarius biffi n. sp., from the eastern Pacific, is described. The species is distinguished from other eastern Pacific species of Notarius by the following features: mouth small (width 34.2-39.3% head length); eye large (diameter 3.8-4.5% standard length); mandibulary barbels short (length 10.2-13.1% standard length); distance between anterior nostrils short (17.9-20.8% head length); caudal peduncle relatively slender (depth 6.1-6.7% SL); gill rakers on the first arch 11-12. N. insculptus (Jordan and Gilbert, 1883) new combination is redescribed herein. This species is distinguished from other eastern Pacific Notarius as follows: highly developed, sculptured epioccipital bones, forming with the supraoccipital a basally wide complex process which tapers drastically posteriorly; supraoccipital process length 0.7-0.9 in the base of the complex process; predorsal plate narrow and crescent-shaped; mouth large (width 45.8-54.8% head length); maxillary barbels long (length 26.7-30.3% standard length). Based on mitochondrial phylogenetic evidence ( combined cytochrome b and ATP synthase 8/6 data set with 1937 base pairs) and general morphology, the amphiamerican genus Notarius is expanded to include a total of 14 species, eight of which are presented as new combinations (N. cookei, N. insculptus, N. kessleri, N. luniscutis, N. neogranatensis, N. phrygiatus, N. quadriscutis, and N. rugispinis). The nomenclatural status of the eastern Pacific ariids Hexanematichthys henni, Arius hassleriana, A. festae, A. labiatus, A. planiceps, and A. osculus is discussed. Finally, a key to identify seven described species of Notarius from the eastern Pacific is presented. C1 Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. Smithsonian Trop Res Inst, Naos Mol Lab, Balboa, Panama. Univ Nacl Colombia, Inst Ciencias Nat, Santa Marta, Colombia. RP Betancur-R, R (reprint author), Auburn Univ, Dept Biol Sci, 331 Funchess, Auburn, AL 36849 USA. EM betanri@auburn.edu; aacero@invemar.org.co RI Betancur-R., Ricardo/A-7276-2009 NR 21 TC 10 Z9 10 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 29 PY 2004 IS 703 BP 1 EP 20 PG 20 WC Zoology SC Zoology GA 877TN UT WOS:000225594300001 ER PT J AU Leverington, DW AF Leverington, DW TI Volcanic rilles, streamlined islands, and the origin of outflow channels on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE channel; Mars; volcanism ID PATHFINDER LANDING SITE; MARTIAN LANDSCAPE; VENUSIAN CHANNELS; CERBERUS FOSSAE; KILAUEA VOLCANO; MANGALA-VALLES; SINUOUS RILLES; MAGELLAN DATA; KASEI VALLES; FLOWING LAVA AB The widely accepted view that catastrophic flow of liquid water was the dominant process involved in formation of outflow channels on Mars has as part of its foundation the assumption that the flow of lava could not have formed Martian features such as streamlined islands and anastamosing channels. However, lunar and Venusian channels, believed to have formed through volcanic processes in the absence of water, are indeed associated with such features. Additionally, many lunar and Venusian rilles head at topographic depressions, a common characteristic of Martian outflow channels. Lunar rilles typically lack positive relief accumulations of volcanic deposits at their mouths, suggesting that contrary to previous assertions, absence of such accumulations at the mouths of Martian outflow channels is not incompatible with a common mode of formation. Consistent with an igneous origin for outflow channels and certain valley systems on Mars, volcanic processes can produce a wide range of landforms that are similar to those normally associated with the flow of water, including channel terraces and complex channel networks. The simplest interpretation of Martian channels that extend from volcanic source regions onto volcanic plains is as conduits formed by the flow of lava. Channel formation hypotheses requiring major changes in Martian atmospheric properties or repeated catastrophic flow of water from volcanic features appear needlessly exotic alongside the igneous hypothesis for channel formation. In light of these points, future investigations of Martian outflow channels should more actively consider volcanic processes as candidate mechanisms for channel formation. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Leverington, DW (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, POB 37012,Room 3774,MRC 0315, Washington, DC 20013 USA. EM leveringtond@nasm.si.edu NR 137 TC 35 Z9 35 U1 1 U2 11 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 OCT 28 PY 2004 VL 109 IS E10 AR E10011 DI 10.1029/2004JE002311 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 868AF UT WOS:000224883500001 ER PT J AU Ruiz-Lapuente, P Comeron, F Mendez, J Canal, R Smartt, SJ Filippenko, AV Kurucz, RL Chornock, R Foley, RJ Stanishev, V Ibata, R AF Ruiz-Lapuente, P Comeron, F Mendez, J Canal, R Smartt, SJ Filippenko, AV Kurucz, RL Chornock, R Foley, RJ Stanishev, V Ibata, R TI The binary progenitor of Tycho Brahe's 1572 supernova SO NATURE LA English DT Article ID IA SUPERNOVAE; REMNANT; SYSTEMS; STARS; MODEL AB The brightness of type Ia supernovae, and their homogeneity as a class, makes them powerful tools in cosmology, yet little is known about the progenitor systems of these explosions. They are thought to arise when a white dwarf accretes matter from a companion star, is compressed and undergoes a thermonuclear explosion(1-3). Unless the companion star is another white dwarf ( in which case it should be destroyed by the mass-transfer process itself), it should survive and show distinguishing properties. Tycho's supernova(4,5) is one of only two type Ia supernovae observed in our Galaxy, and so provides an opportunity to address observationally the identification of the surviving companion. Here we report a survey of the central region of its remnant, around the position of the explosion, which excludes red giants as the mass donor of the exploding white dwarf. We found a type G0 - G2 star, similar to our Sun in surface temperature and luminosity ( but lower surface gravity), moving at more than three times the mean velocity of the stars at that distance, which appears to be the surviving companion of the supernova. C1 Univ Barcelona, Dept Astron, E-08028 Barcelona, Spain. Max Planck Inst Astrophys, D-85748 Garching, Germany. European So Observ, D-85748 Garching, Germany. Isaac Newton Grp, E-38780 Tenerife, Canary Islands, Spain. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stockholm Univ, AlbaNova Univ Ctr, Dept Phys, SE-10891 Stockholm, Sweden. Observ Strasbourg, F-67000 Strasbourg, France. RP Ruiz-Lapuente, P (reprint author), Univ Barcelona, Dept Astron, Marti & Franques 1, E-08028 Barcelona, Spain. EM pilar@am.ub.es RI Stanishev, Vallery/M-8930-2013 OI Stanishev, Vallery/0000-0002-7626-1181 NR 27 TC 141 Z9 143 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 28 PY 2004 VL 431 IS 7012 BP 1069 EP 1072 DI 10.1038/nature03006 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 865VB UT WOS:000224730800032 PM 15510140 ER PT J AU Huang, YM AF Huang, YM TI The subgenus Stegomyia of Aedes in the afrotropical region with keys to the species (Diptera : Culicidae) SO ZOOTAXA LA English DT Review DE mosquitoes; Stegomyia; characteristic; systematics; medical significance; identification; new species; Afrotropical Region ID YELLOW-FEVER; LECTOTYPE DESIGNATION; CHIKUNGUNYA VIRUS; IVORY-COAST; ZIKA VIRUS; AFRICA; ALBOPICTUS; UGANDA; TRANSMISSION; ASSIGNMENT AB The subgenus Stegomyia Theobald of the genus Aedes Meigen in the Afrotropical Region is characterized. Eleven species groups are recognized and diagnosed. The taxonomy, distribution, bionomics and medical importance of the species of the region are discussed and summarized. Keys and illustrations are provided for the identification of the 11 species groups and 59 species and subspecies known to occur in this region. Information on the present status of the species of the African Stegomyia is summarized. Six new species: Aedes ealaensis, ethiopiensis, gandaensis, hogsbackensis, mpusiensis and sampi are recognized. Aedes blacklocki Evans is restored to specific status. One subspecies, denderensis Wolfs is elevated to specific status. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, MRC-534,POB 37012, Washington, DC 20013 USA. EM huang.yiau-min@nmnh.si.edu NR 102 TC 17 Z9 17 U1 3 U2 17 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 27 PY 2004 IS 700 BP 1 EP 120 PG 120 WC Zoology SC Zoology GA 877TK UT WOS:000225593900001 ER PT J AU Jonker, PG Nelemans, G AF Jonker, PG Nelemans, G TI The distances to Galactic low-mass X-ray binaries: consequences for black hole luminosities and kicks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE black hole physics; binaries : close; stars : neutron; X-rays : binaries ID NOVA MUSCAE 1991; PHOTOSPHERIC RADIUS EXPANSION; TRANSIENT XTE J1118+480; OPTICAL LIGHT CURVES; NEUTRON-STAR; GRO J1655-40; CYGNUS X-2; ACCRETION DISC; INTERSTELLAR EXTINCTION; SUPERLUMINAL SOURCE AB We investigated the reported distances of Galactic black hole (BH) and neutron star low-mass X-ray binaries (LMXBs). Comparing the distances derived for the neutron stars Cyg X-2 and XTE J2123-058 using the observed Eddington limited photospheric radius expansion bursts with the distances derived using the observed radius and effective temperature of the companion star, we find that the latter are smaller by approximately a factor of 1.5-2. The latter method is often employed to determine the distance to BH LMXBs. A possible explanation for this discrepancy is that the stellar absorption lines in fast rotating companion stars are different from those in the slowly rotating template stars as was found before for early-type stars. This could lead to a systematic mis-classification of the spectral type of the companion star, which in turn would yield a systematic error in the distance. Further, we derive a distance of 4.0(-1.2)(+2.0) kpc for V404 Cyg, using parameters available in the literature. The interstellar extinction seems to have been overestimated for XTE J1550-564 and possibly for two other BH sources (H 1705-25 and GS 2000+25) as well. As a result of this, the distance to XTE J1550-564 may have been underestimated by as much as a factor three. We find that, using the new distances for XTE J1550-564 and V404 Cyg, the maximum outburst luminosity for at least five, but perhaps even seven, of the 15 BH soft X-ray transients exceed the Eddington luminosity for a 10-M(circle dot) BH-showing that these systems would be classified as ultra-luminous X-ray sources had we observed them in other Galaxies. This renders support for the idea that many ultra-luminous X-ray sources are stellar-mass rather than intermediate-mass BHs. We find that the rms-value of the distance to the Galactic plane for BHs is consistent with that of neutron star LMXBs. This suggests that BHs could also receive a kick-velocity during their formation, although this has to be investigated in more detail. We find that the Galactic neutron star and BH l- and b-distributions are consistent with being the same. The neutron star and BH distribution is asymmetric in l with an excess of systems between -30degrees