Probing The Lower Mass Limit for Supernova Progenitors and the High-Mass End of the Initial-Final Mass Relation from White Dwarfs in the Open Cluster M35 (NGC 2168)We present a photometric and spectroscopic study of the white dwarf population of the populous, intermediate-age open cluster M35 (NGC 2168); this study expands upon our previous study of the white…Kurtis A. Williams, Michael Bolte, Detlev Koester·Nov 10, 2008SaveLearn
Highly ionized gas on galaxy scales: mapping the interacting Seyfert galaxy LEDA 135736We have used the VIMOS IFU to map the properties of the Seyfert 1.9 galaxy LEDA 135736. These maps reveal a number of interesting features including: an Extended Narrow Line Region detectable out to…J. Gerssen, D. J. Wilman, L. Christensen et al.·Nov 10, 2008SaveLearn
High-velocity neon line emission from the ULIRG IRAS F00183-7111: revealing the optically obscured base of a nuclear outflowWe report the first mid-IR detection of highly disturbed ionized gas in the ultraluminous infrared galaxy IRAS F00183-7111. The gas, traced by the 12.81um [NeII] and 15.56um [NeIII] lines, spans a…H. W. W. Spoon, L. Armus, J. A. Marshall et al.·Nov 10, 2008SaveLearn
A Catalog of 24um Sources Toward the Galactic CenterWe present a 1.5deg x 8deg (220pc x 1195pc) Multiband Imaging Photometer for Spitzer 24um image of the Galactic Center and an accompanying point source list. This image is the highest spatial…J. L. Hinz, G. H. Rieke, F. Yusef-Zadeh et al.·Nov 10, 2008SaveLearn
Galaxies appear simpler than expectedGalaxies are complex systems the evolution of which apparently results from the interplay of dynamics, star formation, chemical enrichment, and feedback from supernova explosions and supermassive…M. J. Disney, J. D. Romano, D. A. Garcia-Appadoo et al.·Nov 10, 2008SaveLearn
New biorthogonal potential--density basis functionsWe use the weighted integral form of spherical Bessel functions, and introduce a new analytical set of complete and biorthogonal potential--density basis functions. The potential and density…Alireza Rahmati, Mir Abbas Jalali·Nov 10, 2008SaveLearn
Average Infrared Galaxy Spectra From Spitzer Flux Limited SamplesThe mid-infrared spectroscopic analysis of a flux-limited sample of galaxies with fv(24um) > 10 mJy is presented. Sources observed are taken from the Spitzer First Look Survey (FLS) catalog and from…Daniel W. Weedman, James R. Houck·Nov 10, 2008SaveLearn
The Local Theory of the Cosmic SkeletonThe local theory of the critical lines of 2D and 3D Gaussian fields that underline the cosmic structures is presented. In the context of cosmological matter distribution the subset of critical lines…D. Pogosyan, C. Pichon, C. Gay et al.·Nov 10, 2008SaveLearn
A Modified Stratified Model for 3C 273 JetWe present a modified stratified jet model to interpret the observed spectral energy distributions of knots in 3C 273 jet. Based on the hypothesis of the single index of the particle energy spectrum…Wen-Po Liu, Zhi-Qiang Shen·Nov 10, 2008SaveLearn
Mass transfer dynamics in double degenerate binary systemsWe present a numerical study of the mass transfer dynamics prior to the gravitational wave-driven merger of a double white dwarf system. Recently, there has been some discussion about the dynamics of…M. Dan, S. Rosswog, M. Brüggen·Nov 10, 2008SaveLearn
A Blind Search for Bursts of Very High Enery Gamma Rays with MilagroMilagro is a water-Cherenkov detector that observes the extended air showers produced by cosmic gamma rays of energies E>100GeV. The effective area of Milagro peaks at energies E~10TeV, however it is…Vlasios Vasileiou·Nov 10, 2008SaveLearn
Fermi Acceleration at relativistic ShocksAfter a successful development of theoretical and numerical works on Fermi acceleration at relativistic shocks, some difficulties recently raised with the scattering issue, a crucial aspect of the…Guy Pelletier, Martin Lemoine, A. Marcowith·Nov 10, 2008SaveLearn
XMM-Newton observation of MACHO 104.20906.960: a dwarf nova candidate with a 2 h periodThe binaries known as cataclysmic variables are particular binary systems in which the primary star (a white dwarf) accretes material from a secondary via Roche-lobe mechanism. Usually, these objects…A. A. Nucita, S. Carpano, F. De Paolis et al.·Nov 10, 2008SaveLearn
A variable near-infrared counterpart to the neutron-star low-mass X-ray binary 4U 1705-440We report the discovery of a near-infrared (nIR) counterpart to the persistent neutron-star low-mass X-ray binary 4U 1705-440, at a location consistent with its recently determined Chandra X-ray…Jeroen Homan, David L. Kaplan, Maureen van den Berg et al.·Nov 10, 2008SaveLearn
Cores and Cusps in the Dwarf SpheroidalsWe consider the problem of determining the structure of the dark halo of nearby dwarf spheroidal galaxies (dSphs) from the spherical Jeans equations. Whether the dark halos are cusped or cored at the…N. W. Evans, J. An, M. G. Walker·Nov 10, 2008SaveLearn
A five-wave HLL Riemann solver for relativistic MHDWe present a five-wave Riemann solver for the equations of ideal relativistic magnetohydrodynamics. Our solver can be regarded as a relativistic extension of the five-wave HLLD Riemann solver…A. Mignone, M. Ugliano, G. Bodo·Nov 10, 2008SaveLearn
Masses, Beaming and Eddington Ratios in Ultraluminous X-ray SourcesI suggest that the beaming factor in bright ULXs varies as b m-2, where m is the Eddington ratio for accretion. This is required by the observed universal $L soft…A. R. King·Nov 10, 2008SaveLearn
HCO mapping of the Horsehead : Tracing the illuminated dense molecular cloud surfacesFar-UV photons strongly affect the physical and chemical state of molecular gas in the vicinity of young massive stars. We have obtained maps of the HCO and H13CO+ ground state lines towards the…Maryvonne Gerin, Javier R. Goicoechea, Jérôme Pety et al.·Nov 10, 2008SaveLearn
The XMM-Newton Serendipitous Survey. VI. The X-ray Luminosity FunctionWe present the X-ray luminosity function of AGN in three energy bands (Soft: 0.5-2 keV, Hard: 2-10 keV and Ultrahard: 4.5-7.5 keV). We have used the XMS survey along with other highly complete…J. Ebrero, F. J. Carrera, M. J. Page et al.·Nov 10, 2008SaveLearn
The Globular Cluster Systems in the Coma Ellipticals. IV: WFPC2 Photometry for Five Giant EllipticalsWe analyze photometric data in V and I for the globular cluster (GC) systems in five of the giant ellipticals in the Coma Cluster: NGC 4874, 4881, 4889, 4926, and IC 4051. We find that the GC…W. E. Harris, J. J. Kavelaars, D. A. Hanes et al.·Nov 10, 2008SaveLearn
Seismology of beta Cephei stars: differentially-rotating models for interpreting the oscillation spectrum of nu-EridaniA method for the asteroseismic analysis of beta Cephei stars is presented and applied to the star nu Eridani. The method is based on the analysis of rotational splittings, and their asymmetries using…J. C. Suarez, A. Moya, P. J. Amado et al.·Nov 10, 2008SaveLearn
The effect of stellar feedback on the formation and evolution of gas and dust tori in AGNRecently, the existence of geometrically thick dust structures in Active Galactic Nuclei (AGN) has been directly proven with the help of mid-infrared interferometry. The observations are consistent…M. Schartmann, K. Meisenheimer, H. Klahr et al.·Nov 10, 2008SaveLearn
Supernova Remnants in the AKARI IRC Survey of the Large Magellanic CloudWe present the near- to mid-infared study of supernova remnants (SNRs) using the AKARI IRC Survey of the Large Magellanic Cloud (LMC). The LMC survey observed about a 10 square degree area of the LMC…Ji Yeon Seok, Bon-Chul Koo, Takashi Onaka et al.·Nov 10, 2008SaveLearn
Magnetic Fields and the Polarization of Astrophysical Maser Radiation: A ReviewBasic aspects of the relationship between the magnetic field and polarized maser radiation are described with the emphasis on interpreting the observed spectra. Special attention is given to three…William D. Watson·Nov 10, 2008SaveLearn
Testing the Possible Intrinsic Origin of the Excess of Very Strong MgII Absorbers Along GRB Lines-of-SightThe startling discovery of Prochter et al. (2006) that the frequency of very strong (Wr(2796)>1 A) MgII absorbers along gamma-ray burst (GRB) lines of sight ([dN/dz]GRB = 0.90) is more than three…A. Cucchiara, T. Jones, J. C. Charlton et al.·Nov 9, 2008SaveLearn