Probing the kinematics of early-type galaxy halos using planetary nebulaeWe present first results of a study of the halo kinematics for a sample of early type galaxies using planetary nebulae (PNe) as kinematical tracers. PNe allow to extend up to several effective radii…L. Coccato, O. Gerhard, M. Arnaboldi et al.·Nov 14, 2008SaveLearn
Aspect angle for interstellar magnetic field in SN 1006A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between…O. Petruk, G. Dubner, G. Castelletti et al.·Nov 14, 2008SaveLearn
The AGN nature of three INTEGRAL sources: IGR J18249-3243, IGR J19443+2117 and IGR J22292+6647The third INTEGRAL/IBIS survey has revealed several new hard X-ray sources, which are still unclassified. To identify these sources, we need to find their counterparts at other wavelengths and then…R. Landi, J. B. Stephen, N. Masetti et al.·Nov 14, 2008SaveLearn
Prediction of Solar Flares from a Statistical Analysis of Events during Solar Cycle 23Ways to give medium- and short-term predictions of solar flares are proposed according to the statistical analysis of events during solar cycle 23. On one hand, the time distribution of both C and M…Z. Q. Qu·Nov 14, 2008SaveLearn
Flaring variability of MicroquasarsWe discuss flaring variability of radio emission of microquasars, measured in monitoring programs with the RATAN-600 radio telescope. We carried out a multi-frequency (1-30 GHz) daily monitoring of…Sergei A. Trushkin, Nikolaj N. Bursov, Nikolaj A. Nizhelskij·Nov 14, 2008SaveLearn
Six Hot Topics in Planetary AstronomySix hot topics in modern planetary astronomy are described: 1) lightcurves and densities of small bodies 2) colors of Kuiper belt objects and the distribution of the ultrared matter 3) spectroscopy…David Jewitt·Nov 14, 2008SaveLearn
The timescales of chemical enrichment in the GalaxyThe time-scales of chemical enrichment are fundamental to understand the evolution of abundances and abundance ratios in galaxies. In particular, the time-scales for the enrichment by SNe II and SNe…Antonio Pipino, Francesca Matteucci·Nov 14, 2008SaveLearn
Exploring Parameter Constraints on Quintessential Dark Energy: the Inverse Power Law ModelWe report on the results of a Markov Chain Monte Carlo (MCMC) analysis of an inverse power law (IPL) quintessence model using the Dark Energy Task Force (DETF) simulated data sets as a representation…Mark Yashar, Brandon Bozek, Augusta Abrahamse et al.·Nov 14, 2008SaveLearn
Lorentz Invariance Violation and the Observed Spectrum of Ultrahigh Energy Cosmic RaysThere has been much interest in possible violations of Lorentz invariance, particularly motivated by quantum gravity theories. It has been suggested that a small amount of Lorentz invariance…S. T. Scully, F. W. Stecker·Nov 13, 2008SaveLearn
The Race Between Stars and Quasars in Reionizing Cosmic HydrogenThe cosmological background of ionizing radiation has been dominated by quasars once the Universe aged by ~2 billion years. At earlier times (redshifts z>3), the observed abundance of bright quasars…Abraham Loeb·Nov 13, 2008SaveLearn
The local FIR Galaxy Colour-Luminosity distribution: A reference for BLAST, and Herschel/SPIRE sub-mm surveysWe measure the local galaxy far-infrared (FIR) 60-to-100 um colour-luminosity distribution using an all-sky IRAS survey. This distribution is an important reference for the next generation of…Edward L. Chapin, David H. Hughes, Itziar Aretxaga·Nov 13, 2008SaveLearn
Massive, red galaxies in a hierarchical universe I. Counts of Extremely Red Objects and basic propertiesWe present predictions for the abundance and nature of Extremely Red Objects (EROs) in the Lambda cold dark matter model. EROs are red, massive galaxies observed at z>= 1 and their numbers and…V. Gonzalez-Perez, C. M. Baugh, C. G. Lacey et al.·Nov 13, 2008SaveLearn
Fomalhaut's Debris Disk and Planet: Constraining the Mass of Fomalhaut b From Disk MorphologyFollowing the optical imaging of the exoplanet candidate Fomalhaut b (Fom b), we present a numerical model of how Fomalhaut's debris disk is gravitationally shaped by an interior planet. The…E. Chiang, E. Kite, P. Kalas et al.·Nov 13, 2008SaveLearn
The cosmology dependence of weak lensing cluster countsWe present the main results of a numerical study of weak lensing cluster counting. We examine the scaling with cosmology of the projected-density-peak mass function. Our main conclusion is that the…Laura Marian, Robert E. Smith, Gary M. Bernstein·Nov 13, 2008SaveLearn
Non-Gaussian Signatures from the Postinflationary Early UniverseWe consider contributions to non-Gaussianity of the Cosmic Microwave Background (CMB) from remnants of post-inflationary phase transitions in the very early universe. Such signatures can…Alessandra Silvestri, Mark Trodden·Nov 13, 2008SaveLearn
Extremely Red Objects in a hierarchical universeWe analyse whether hierarchical formation models based on Lambda cold dark matter cosmology can produce enough massive red galaxies to match observations. For this purpose, we compare with…V. Gonzalez-Perez, C. M. Baugh, C. G. Lacey et al.·Nov 13, 2008SaveLearn
Optical Images of an Exosolar Planet 25 Light Years from EarthFomalhaut is a bright star 7.7 parsecs (25 light years) from Earth that harbors a belt of cold dust with a structure consistent with gravitational sculpting by an orbiting planet. Here, we present…Paul Kalas, James R. Graham, Eugene Chiang et al.·Nov 13, 2008SaveLearn
Alignment between galaxies and large-scale structureBased on the Sloan Digital Sky Survey DR6 (SDSS) and Millennium Simulation (MS) we investigate the alignment between galaxies and large-scale structure. For this purpose we develop two new…A. Faltenbacher, Cheng Li, Simon D. M. White et al.·Nov 13, 2008SaveLearn
On the importance of satellite lines to the He-like K ALPHA complex and the G ratio for calcium, iron, and nickelNew, more detailed calculations of the emission spectra of the He-like K ALPHA complex of calcium, iron and nickel have been carried out using data from both distorted-wave and R-matrix calculations.…J. Oelgoetz, C. J. Fontes, H. L. Zhang et al.·Nov 13, 2008SaveLearn
CARS: the CFHTLS-Archive-Research Survey; I. Five-band multi-colour data from 37 sq. deg. CFHTLS-Wide observationsWe present the CFHTLS-Archive-Research Survey (CARS). It is a virtual multi-colour survey based on public archive images from the CFHT-Legacy-Survey. Our main scientific interests in CARS are optical…T. Erben, H. Hildebrandt, M. Lerchster et al.·Nov 13, 2008SaveLearn
On the Origin of Dwarf Elliptical Galaxies: The Fundamental PlaneEarly-type dwarf galaxies are the most common type of galaxies observed in the Universe. The origin of this kind of systems is still not well understood. The aim of this paper is to investigate…J. A. L. Aguerri, C. Gonzalez-Garcia·Nov 13, 2008SaveLearn
Primordial non-Gaussianities in the Intergalactic MediumWe present results from the first high-resolution hydrodynamical simulations of non-Gaussian cosmological models. We focus on the statistical properties of the transmitted Lyman-alpha flux in the…M. Viel, E. Branchini, K. Dolag et al.·Nov 13, 2008SaveLearn
Constraints on the Primordial Magnetic Field from σ8A primordial magnetic field (PMF) can affect the evolution of density field fluctuations in the early universe.In this paper we constrain the PMF amplitude Bλ and power spectral index…Dai G. Yamazaki, Kiyotomo Ichiki, Toshitaka Kajino et al.·Nov 13, 2008SaveLearn
Spatially Resolved 3 micron Spectroscopy of Elias 1: Origin of Diamonds in Protoplanetary DisksWe present spatially resolved 3 um spectra of Elias 1 obtained with an adaptive optics system. The central part of the disk is almost devoid of PAH emission at 3.3 um; it shows up only at 30 AU and…M. Goto, Th. Henning, A. Kouchi et al.·Nov 13, 2008SaveLearn
Reconstructing mass profiles of simulated galaxy clusters by combining Sunyaev-Zeldovich and X-ray imagesWe present a method to recover mass profiles of galaxy clusters by combining data on thermal Sunyaev-Zeldovich (tSZ) and X-ray imaging, thereby avoiding to use any information on X-ray spectroscopy.…S. Ameglio, S. Borgani, E. Pierpaoli et al.·Nov 13, 2008SaveLearn