Variation of fluxes of RR Tel emission lines measured in 2000 with respect to 1996The aim of this work is to make available unpublished non-Fe+ emission line fluxes from optical spectra of the symbiotic nova RR Tel which were taken in 2000, and to compare them with fluxes of the…D. Kotnik-Karuza, M. Friedjung, K. Exter·Nov 27, 2008SaveLearn
Influence of the photon - neutrino processes on magnetar coolingThe photon-neutrino processes γe e ν ν, γ ν ν and γγ ν ν are investigated in the presence of a strongly magnetized and dense electron-positron plasma. The…M. V. Chistyakov, D. A. Rumyantsev·Nov 27, 2008SaveLearn
Semi-analytical formulas for the Hertzsprung-Russell DiagramThe absolute visual magnitude as function of the observed colour (B-V), also named Hertzsprung-Russell diagram can be described through five equations; that in presence of calibrated stars means…Lorenzo Zaninetti·Nov 27, 2008SaveLearn
Invariant manifolds and the response of spiral arms in barred galaxiesThe unstable invariant manifolds of the short-period family of periodic orbits around the unstable Lagrangian points L1 and L2 of a barred galaxy define loci in the configuration space which…P. Tsoutsis, C. Kalapotharakos, C. Efthymiopoulos et al.·Nov 27, 2008SaveLearn
Synchrotron Radiation from the Galactic Center in Decaying Dark Matter ScenarioWe discuss the synchrotron radiation flux from the Galactic center in unstable dark matter scenario. Motivated by the anomalous excess of the positron fraction recently reported by the PAMELA…Koji Ishiwata, Shigeki Matsumoto, Takeo Moroi·Nov 27, 2008SaveLearn
A correlation between spin parameter and dark matter halo massUsing a set of high-resolution dark matter only cosmological simulations we found a correlation between the dark matter halo mass M and its spin parameter lambda for objects forming at redshifts z >…Alexander Knebe, Chris Power·Nov 27, 2008SaveLearn
On the nature of faint Low Surface Brightness galaxies in the Coma clusterThis project is the continuation of our study of faint Low Surface Brightness Galaxies (fLSBs) in one of the densest nearby galaxy regions known, the Coma cluster. Our goal is to improve our…C. Adami, R. Pello, M. P. Ulmer et al.·Nov 27, 2008SaveLearn
Ironing out primordial temperature fluctuations with polarisation: optimal detection of cosmic structure imprintsSecondary anisotropies of the cosmic microwave background (CMB) can be detected by using the cross-correlation between the large-scale structure (LSS) and the CMB temperature fluctuations. In such…Mona Frommert, Torsten A. Ensslin·Nov 26, 2008SaveLearn
Three dimensional magnetic field structure of six parsec-scale active galactic nuclei jetsThe parsec-scale Faraday rotation measure (RM) distribution of six "blazars" is investigated using multi-frequency (4.6--43 GHz) polarization observations taken on 2006 July 2 with the VLBA.…Shane P. O'Sullivan, Denise C. Gabuzda·Nov 26, 2008SaveLearn
On the possibility of primary identification of individual cosmic ray showersThe transition between the Galactic and extragalactic cosmic ray components could take place either in the region of the spectrum known as the second knee or in the ankle. There are several models of…A. D. Supanitsky, G. Medina-Tanco, A. Etchegoyen·Nov 26, 2008SaveLearn
Quantum Coherence of Relic NeutrinosWe argue that in at least a portion of the history of the universe the relic background neutrinos are spatially-extended, coherent superpositions of mass states. We show that an appropriate quantum…George M. Fuller, Chad T. Kishimoto·Nov 26, 2008SaveLearn
Gamma-ray luminosity function of Gamma-ray bright AGNsDetection of Gamma-ray emission from a class of active galactic nuclei (viz blazars), has been one of the important findings from the Compton Gamma Ray Observatory (CGRO). However, their Gamma-ray…D. Bhattacharya, P. Sreekumar, R. Mukherjee·Nov 26, 2008SaveLearn
Analytical Blowup Solutions to the Pressureless Navier-Stokes-Poisson Equations with Density-dependent Viscosity in RNWe study the N-dimensional pressureless Navier--Stokes-Poisson equations with density-dependent viscosity. With the extension of the blowup solutions for the Euler-Poisson equations, the analytical…Manwai Yuen·Nov 26, 2008SaveLearn
Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditionsWe perform a series of high-resolution N-body simulations of cosmological structure formation starting from Gaussian and non-Gaussian initial conditions. We adopt the best-fitting cosmological…Annalisa Pillepich, Cristiano Porciani, Oliver Hahn·Nov 26, 2008SaveLearn
Probing the Primordial Power Spectrum with Cluster Number CountsWe investigate how well galaxy cluster number counts can constrain the primordial power spectrum. Measurements of the primary anisotropies in the cosmic microwave background (CMB) may be limited, by…Teeraparb Chantavat, Christopher Gordon, Joseph Silk·Nov 26, 2008SaveLearn
Matter density perturbations in modified gravity models with arbitrary coupling between matter and geometryWe consider theories with an arbitrary coupling between matter and gravity and obtain the perturbation equation of matter on subhorizon scales. Also, we derive the effective gravitational constant…Savvas Nesseris·Nov 26, 2008SaveLearn
Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Bayesian Estimation of CMB Polarization MapsWe describe a sampling method to estimate the polarized CMB signal from observed maps of the sky. We use a Metropolis-within-Gibbs algorithm to estimate the polarized CMB map, containing Q and U…J. Dunkley, D. N. Spergel, E. Komatsu et al.·Nov 26, 2008SaveLearn
Results of MAGIC on Galactic sourcesMAGIC is a single-dish Cherenkov telescope located on La Palma (Spain), hence with an optimal view on the Northern sky. Sensitive in the 30 GeV-30 TeV energy band, it is nowadays the only…Javier Rico·Nov 26, 2008SaveLearn
The Adaptive TreePM: An Adaptive Resolution Code for Cosmological N-body SimulationsCosmological N-Body simulations are used for a variety of applications. Indeed progress in the study of large scale structures and galaxy formation would have been very limited without this tool. For…J. S. Bagla, Nishikanta Khandai·Nov 26, 2008SaveLearn
MASSCLEAN - MASSive CLuster Evolution and ANalysis Package - Description and TestsWe present MASSCLEAN, a new, sophisticated and robust stellar cluster image and photometry simulation package. This visualization tool is able to create color-magnitude diagrams and standard FITS…Bogdan Popescu, M. M. Hanson·Nov 26, 2008SaveLearn
Morphological Composition of z~0.4 groups: The site of S0 formationThe low redshift Universe (z<~0.5) is not a dull place. Processes leading to the suppression of star formation and morphological transformation are prevalent: this is particularly evident in the…D. J. Wilman, A. Oemler, J. S. Mulchaey et al.·Nov 26, 2008SaveLearn
Spectroscopy of High-Redshift Supernovae from the ESSENCE Project: The First Four YearsWe present the results of spectroscopic observations from the ESSENCE high-redshift supernova (SN) survey during its first four years of operation. This sample includes spectra of all SNe Ia whose…R. J. Foley, T. Matheson, S. Blondin et al.·Nov 26, 2008SaveLearn
Kinematics of the Young Stellar Objects associated with the Cometary Globules in the Gum NebulaAn analysis of proper motion measurements of the Young Stellar Objects (YSOs) associated with the Cometary Globules (CGs) in the Gum Nebula is presented. While earlier studies based on the radial…Rumpa Choudhury, H. C. Bhatt·Nov 26, 2008SaveLearn
The Megamaser Cosmology Project: I. VLBI observations of UGC 3789The Megamaser Cosmology Project (MCP) seeks to measure the Hubble Constant (Ho) in order to improve the extragalactic distance scale and constrain the nature of dark energy. We are searching for…M. J. Reid, J. A. Braatz, J. J. Condon et al.·Nov 26, 2008SaveLearn
The VLBI morphology of M81* at 43 GHzThe radio source M81* at the core of the nearby spiral galaxy M81 is a low-luminosity active galactic nucleus. The close distance of 3.63Mpc allows its morphology to be studied in great detail. Here…Eduardo Ros, Miguel-Angel Perez-Torres·Nov 26, 2008SaveLearn