The Co-Evolution of Galaxies and Black Holes: Current Status and Future ProspectsI begin by summarizing the evidence that there is a close relationship between the evolution of galaxies and supermassive black holes. They evidently share a common fuel source, and feedback from the…T. M. Heckman·Sep 5, 2008SaveLearn
An improved limit on the neutrino mass with CMB and redshift-dependent halo bias-mass relations from SDSS, DEEP2, and Lyman-Break GalaxiesWe use measurements of luminosity-dependent galaxy bias at several different redshifts, SDSS at z=0.05, DEEP2 at z=1 and LBGs at z=3.8, combined with WMAP five-year cosmic microwave background…Francesco De Bernardis, Paolo Serra, Asantha Cooray et al.·Sep 5, 2008SaveLearn
Efficient Power Spectrum Estimation for High Resolution CMB MapsEstimation of the angular power spectrum of the Cosmic Microwave Background (CMB) on a small patch of sky is usually plagued by serious spectral leakage, specially when the map has a hard edge. Even…Sudeep Das, Amir Hajian, David N. Spergel·Sep 5, 2008SaveLearn
Practical cosmology and cosmological physicsWe present a summary of the International conference "Problems of practical cosmology", held at Russian Geographical Society, 23-27 June 2008, St.-Petersburg, Russia, where original reports…Yu. Baryshev, I. Taganov, P. Teerikorpi·Sep 5, 2008SaveLearn
INTEGRAL sources: from obscured high mass X-ray binaries to supergiant fast X-ray transientsA new type of high-energy binary system has been revealed by the INTEGRAL satellite. These sources are being unveiled by means of multi-wavelength optical, near- and mid-infrared observations. Among…S. Chaty·Sep 5, 2008SaveLearn
Dynamical Constraints on The Masses of the Nuclear Star Cluster and Black Hole in the Late-Type Spiral Galaxy NGC 3621NGC 3621 is a late-type (Sd) spiral galaxy with an active nucleus, previously detected through mid-infrared [Ne V] line emission. Archival Hubble Space Telescope (HST) images reveal that the galaxy…A. J. Barth, L. E. Strigari, M. C. Bentz et al.·Sep 5, 2008SaveLearn
A low-redshift galaxy cluster X-ray Temperature Function incorporating Suzaku dataWe present the first results of a survey of 14 low redshift galaxy clusters using Suzaku. Although luminous (Lx> 1× 1043 erg s-1 (0.1-2.4 keV)), these clusters have no prior pointed X-ray…Cien Shang, Caleb Scharf·Sep 5, 2008SaveLearn
A Full Year's Chandra Exposure on SDSS Quasars from the Chandra Multiwavelength ProjectWe study the spectral energy distributions and evolution of a large sample of optically selected quasars from the Sloan Digital Sky Survey (SDSS) that were observed in 323 Chandra images analyzed by…Paul J. Green, T. L. Aldcroft, G. T. Richards et al.·Sep 5, 2008SaveLearn
The Wide-Field X and Gamma-Ray Telescope ECLAIRs aboard the Gamma-Ray Burst Multi-Wavelength Space Mission SVOMThe X and Gamma-ray telescope ECLAIRs is foreseen to be launched on a low Earth orbit (h=630 km, i=30 degrees) aboard the SVOM satellite (Space-based multi-band astronomical Variable Objects…P. Mandrou, S. Schanne, B. Cordier et al.·Sep 5, 2008SaveLearn
Two Jupiter-Mass Planets Orbiting HD 154672 and HD 205739We report the detection of the first two planets from the N2K Doppler planet search program at the Magellan telescopes. The first planet has a mass of M sin i = 4.96 MJup and is orbiting the G3 IV…Mercedes Lopez-Morales, R. Paul Butler, Debra A. Fischer et al.·Sep 5, 2008SaveLearn
Galaxy mergers at high resolution: From elliptical galaxies to tidal dwarfs and globular clustersNumerical simulations of galaxy mergers are a powerful tool to study these fundamental events in the hierarchical built-up of galaxies. Recent progress have been made owing to improved modeling,…F. Bournaud, M. Bois, E. Emsellem et al.·Sep 5, 2008SaveLearn
Flares in Gamma Ray BurstsThe flare activity that is observed in GRBs soon after the prompt emission with the XRT (0.3-10 KeV) instrument on board of the Swift satellite is leading to important clues in relation to the…G. Chincarini, J. Mao, F. Pasotti et al.·Sep 5, 2008SaveLearn
Gravitational lensing by gravitational wavesGravitational lensing by gravitational wave is considered. We notice that although final and initial direction of photons coincide, displacement between final and initial trajectories occurs. This…G. S. Bisnovatyi-Kogan, O. Yu. Tsupko·Sep 5, 2008SaveLearn
Low-resolution spectroscopy and spectral energy distributions of selected sources towards sigma OrionisAims: We investigated in detail nine sources in the direction of the young sigma Orionis cluster, which is considered a unique site for studying stellar and substellar formation. The nine sources…J. A. Caballero, L. Valdivielso, E. L. Martin et al.·Sep 5, 2008SaveLearn
CMB Anisotropy Induced by a Moving Straight Cosmic StringWe showed that the part of strings could be detected by optical method is only 20% from the total available amount of such objects, therefore the gravitational lensing method has to be…O. S. Sazhina, M. V. Sazhin, V. N. Sementsov et al.·Sep 5, 2008SaveLearn
New deep XMM-Newton observations to the west of the sigma Orionis clusterAims: The objective of this study is to determine the general X-ray properties of the young stars in the external regions of the sigma Orionis cluster (tau ~ 3 Ma, d ~ 385 pc) and yield constraints…J. Lopez-Santiago, J. A. Caballero·Sep 5, 2008SaveLearn
Dehydrogenated polycyclic aromatic hydrocarbons and UV bumpRecent calculations have shown that the UV bump at about 217.5 nm in the extinction curve can be explained by a complex mixture of PAHs in several charge states. Other studies proposed that the…G. Malloci, G. Mulas, C. Cecchi-Pestellini et al.·Sep 5, 2008SaveLearn
The UV luminosity function and star formation rate of the Coma clusterWe present estimates of the GALEX NUV and FUV luminosity functions (LFs) of the Coma cluster, over a total area of ~9 deg2 (~25 Mpc2), i.e. from the cluster center to the virial radius. Our…L. Cortese, G. Gavazzi, A. Boselli·Sep 5, 2008SaveLearn
Mapping dust column density in dark clouds by using NIR scattered light : Case of the Lupus 3 dark cloudWe present a method of mapping dust column density in dark clouds by using near-infrared scattered light. Our observations of the Lupus 3 dark cloud indicate that there is a well defined relation…Yasushi Nakajima, Ryo Kandori, Motohide Tamura et al.·Sep 5, 2008SaveLearn
Searching for the metal-weak thick disc in the solar neighbourhoodAn abundance analysis is presented of 60 metal-poor stars drawn from catalogues of nearby stars provided by Ariyanto et al. (2005) and Schuster et al. (2006). In an attempt to isolate a sample of…Bacham E. Reddy, David L. Lambert·Sep 5, 2008SaveLearn
Vector magnetic fields of Solar GranulationObservations of quiet Sun from the Solar Optical Telescope/Spectro-Polarimeter (SOT/SP) aboard the Hinode spacecraft would reveal the magnetic characters of the solar photosphere. By making use of…Chunlan Jin, Jingxiu Wang, Meng Zhao·Sep 5, 2008SaveLearn
Applications of Bayesian Probability Theory in AstrophysicsBayesian Inference is a powerful approach to data analysis that is based almost entirely on probability theory. In this approach, probabilities model uncertainty rather than randomness or…Brendon J. Brewer·Sep 5, 2008SaveLearn
A Search for Z=-1 Dark Matter Annihilation Products in Cosmic Rays with AMS-01The majority of mass in the universe has not been observed optically and is termed dark matter. The supersymmetric neutralino provides an interesting dark matter candidate, which may self-annihilate…Gray Rybka·Sep 5, 2008SaveLearn
Anomalous CMB north-south asymmetrySeveral accurate analyses have revealed a statistically significant North-South ecliptic asymmetry in the large-angle correlations strength of the Cosmic Microwave Background (CMB) radiation…Armando Bernui·Sep 5, 2008SaveLearn
The Aquarius Project: the subhalos of galactic halosWe have performed the largest ever particle simulation of a Milky Way-sized dark matter halo, and present the most comprehensive convergence study for an individual dark matter halo carried out thus…Volker Springel, Jie Wang, Mark Vogelsberger et al.·Sep 5, 2008SaveLearn