Technology Section of the White Paper on the Status and Future of Ground-based TeV Gamma-ray AstronomyThis is a report on the findings of the technology working group for the white paper on the status and future of TeV gamma-ray astronomy. The white paper is an APS commissioned document, and the…K. Byrum, J. Buckley, S. Bugayov et al.·Oct 24, 2008SaveLearn
The Impact of Non-Gaussian Errors on Weak Lensing SurveysThe weak lensing power spectrum carries cosmological information via its dependence on the growth of structure and on geometric factors. Since much of the cosmological information comes from scales…Masahiro Takada, Bhuvnesh Jain·Oct 23, 2008SaveLearn
On the central core in MHD winds and jetsWe demonstrate that the 1D cylindrical version of the Grad-Shafranov equation is more rich than classical self-similar ones, and more suitable for the astrophysical jets we observe. In particular, it…V. S. Beskin, E. E. Nokhrina·Oct 23, 2008SaveLearn
Overview of the lithium problem in metal-poor stars and new results on 6LiTwo problems are discussed here. The first one is the 0.4 dex discrepancy between the 7Li abundance derived from the spectra of metal-poor halo stars on the one hand, and from Big Bang…Roger Cayrel, Matthias Steffen, Piercarlo Bonifacio et al.·Oct 23, 2008SaveLearn
Global shallow water magnetohydrodynamic waves in the solar tachoclineWe derive analytical solutions and dispersion relations of global magnetic Poincaré (magneto-gravity) and magnetic Rossby waves in the approximation of shallow water magnetohydrodynamics. The…T. V. Zaqarashvili, R. Oliver, J. L. Ballester·Oct 23, 2008SaveLearn
Interchanging Interactive 3-d Graphics for AstronomyWe demonstrate how interactive, three-dimensional (3-d) scientific visualizations can be efficiently interchanged between a variety of mediums. Through the use of an appropriate interchange format,…C. J. Fluke, D. G. Barnes, N. T. Jones·Oct 23, 2008SaveLearn
Turbulence in Wind-Blown Bubbles around Massive StarsWinds from massive stars (> 8 solar masses) result in the formation of wind-blown "bubbles" around these stars. In this paper we study, via two-dimensional numerical hydrodynamic simulations, the…Vikram V Dwarkadas·Oct 23, 2008SaveLearn
Variability of the methane trapping in martian subsurface clathrate hydratesRecent observations have evidenced traces of methane CH4 heterogeneously distributed in the martian atmosphere. However, because the lifetime of CH4 in the atmosphere of Mars is estimated to be…Caroline Thomas, Olivier Mousis, Sylvain Picaud et al.·Oct 23, 2008SaveLearn
The Age and Metallicity of the Bootes I SystemWe present Washington photometry of a field central to the Bootes I dwarf spheroidal galaxy, which was discovered as a stellar overdensity in the Sloan Digital Sky Survey (DR5). We show that the…Joanne Hughes, George Wallerstein, Anne Bossi·Oct 23, 2008SaveLearn
On the Formation and Evolution of cD GalaxiesThe cannibalism mechanism of formation of cD galaxies in clusters of Bautz-Morgan class I is analyzed. Dependences between absolute magnitude of cD galaxies, and of the clusters in which they reside…Hrant Tovmassian·Oct 23, 2008SaveLearn
The luminosity function of galaxies to MBgVriz -14 in z 0.3 clustersWe present deep composite luminosity functions in B, g, V, r, i and z for six clusters at 0.14 < z < 0.40 observed with the Hubble Space Telescope Advanced Camera for Surveys. The…Daniel Harsono, Roberto De Propris·Oct 23, 2008SaveLearn
Dissecting the Red Sequence--I. Star Formation Histories of Quiescent Galaxies: The Color-Magnitude vs. the Color-Sigma RelationWe use a sample of ~16,000 non-emission line galaxies from the SDSS to investigate the physical parameters underlying the well-known color-magnitude and color-sigma relations. Galaxies are sorted in…Genevieve J. Graves, S. M. Faber, Ricardo P. Schiavon·Oct 23, 2008SaveLearn
Reducing the gravitational lensing scatter of Type Ia supernovae without introducing any extra biasMagnification and de-magnification due to gravitational lensing will contribute to the brightness scatter of Type Ia supernovae (SNe Ia). The purpose of this paper is to investigate the possibility…Jakob Jonsson, Edvard Mortsell, Jesper Sollerman·Oct 23, 2008SaveLearn
Matter Power Spectrum for the Generalized Chaplygin Gas Model: The Newtonian ApproachWe model the cosmic medium as the mixture of a generalized Chaplygin gas and a pressureless matter component. Within a neo-Newtonian approach (in which, different from standard Newtonian cosmology,…J. C. Fabris, S. V. B. Goncalves, H. E. S. Velten et al.·Oct 23, 2008SaveLearn
Gravitational waves in vector inflationWe discuss the gravitational waves (GW) in the context of vector inflation. We derive the action for tensor perturbations and find that tachyonic instabilities are present in most (but not all) of…Alexey Golovnev, Viatcheslav Mukhanov, Vitaly Vanchurin·Oct 23, 2008SaveLearn
Probing the Galactic cosmic ray flux with submillimeter and gamma ray dataThe study of Galactic diffuse γ radiation combined with the knowledge of the distribution of the molecular hydrogen in the Galaxy offers a unique tool to probe the cosmic ray flux in the Galaxy. A…S. Casanova, S. Gabici, F. A. Aharonian et al.·Oct 23, 2008SaveLearn
A low-frequency radio halo associated with a cluster of galaxiesClusters of galaxies are the largest gravitationally bound objects in the Universe, containing about 1015 solar masses of hot (108 K) gas, galaxies and dark matter in a typical volume of about 10…G. Brunetti, S. Giacintucci, R. Cassano et al.·Oct 23, 2008SaveLearn
Polarization from the Structured Envelopes of Cool Evolved StarsWe present preliminary calculations of electron scattering polarizations from models of structured cool star envelopes. We note that net polarizations from unresolved sources can result from…R Ignace, G D Henson, J Carson·Oct 23, 2008SaveLearn
Results of WEBT, VLBA and RXTE monitoring of 3C 279 during 2006-2007We present radio-to-optical data taken by the WEBT, supplemented by VLBA and RXTE observations, of 3C 279. Our goal is to use this extensive database to draw inferences regarding the physics of the…V. M. Larionov, S. G. Jorstad, A. P. Marscher et al.·Oct 23, 2008SaveLearn
Dependence of cosmic shear covariances on cosmology - Impact on parameter estimationIn cosmic shear likelihood analyses the covariance is most commonly assumed to be constant in parameter space. Therefore, when calculating the covariance matrix (analytically or from simulations),…Tim Eifler, Peter Schneider, Jan Hartlap·Oct 23, 2008SaveLearn
Dynamical Simulations of Magnetically Channeled Line-Driven Stellar Winds: III. Angular Momentum Loss and Rotational SpindownWe examine the angular momentum loss and associated rotational spindown for magnetic hot stars with a line-driven stellar wind and a rotation-aligned dipole magnetic field. Our analysis here is based…Asif ud-Doula, Stanley P. Owocki, Richard H. D. Townsend·Oct 23, 2008SaveLearn
Light pollution in Spain. An european perspectiveSpain appears in light pollution maps as a country less polluted than their neighbours in the European Union. This seems to be an illusion due to its low population density. The data indicate that…Alejandro Sanchez de Miguel, Jaime Zamorano·Oct 23, 2008SaveLearn
Finding SDSS BALQSOs Using Non-Negative Matrix FactorisationModern spectroscopic databases provide a wealth of information about the physical processes and environments associated with astrophysical populations. Techniques such as blind source separation…James T. Allen, Paul C. Hewett, Vasily Belokurov et al.·Oct 23, 2008SaveLearn
How do f-mode Frequencies Change with Solar Radius?We test the relation between relative f-mode frequency variation and Lagrangian perturbation in the solar radius obtained by Dziembowski and Goode (2004) using several pairs of solar models and show…Piyali Chatterjee, H M. Antia·Oct 23, 2008SaveLearn
WSRT Faraday tomography of the Galactic ISM at λ~ 0.86 mWe investigate the properties of the Galactic ISM by applying Faraday tomography to a radio polarization data set in the direction of the Galactic anti-centre. We address the problem of missing…D. H. F. M. Schnitzeler, P. Katgert, A. G. de Bruyn·Oct 23, 2008SaveLearn