Alignments of Group Galaxies with Neighboring GroupsUsing a sample of galaxy groups found in the Sloan Digital Sky Survey Data Release 4, we measure the following four types of alignment signals: (1) the alignment between the distributions of the…Yougang Wang, Changbom Park, Xiaohu Yang et al.·Oct 19, 2008SaveLearn
Status report of the NuMoon experimentWe show that at wavelengths comparable to the length of the shower produced by an Ultra-High Energy cosmic ray or neutrino, radio signals are an extremely efficient way to detect these particles.…O. Scholten, S. Buitink, J. Bacelar et al.·Oct 19, 2008SaveLearn
Time-series Spectroscopy and Photometry of the Pulsating Subdwarf B Star PG 1219+534 (KY UMa)We present observations and analysis of time-series spectroscopy and photometry of the pulsating subdwarf B star PG 1219+534 (KY UMa). Subdwarf B stars are blue horizontal branch stars which have…M. D. Reed, J. R. Eggen, S. L. Harms et al.·Oct 19, 2008SaveLearn
HELAS Local Helioseismology ActivitiesThe main goals of the HELAS local helioseismology network activity are to consolidate this field of research in Europe, to organise scientific workshops, and to facilitate the distribution of…Hannah Schunker, Laurent Gizon·Oct 19, 2008SaveLearn
Molecular Gas in a Submillimeter Galaxy at z=4.5: Evidence for a Major Merger at 1 Billion Years after the Big BangWe report the detection of CO molecular line emission in the z=4.5 millimeter-detected galaxy COSMOSJ100054+023436 (hereafter: J100+0234) using the IRAM Plateau de Bure interferometer (PdBI) and…E. Schinnerer, C. L. Carilli, P. Capak et al.·Oct 19, 2008SaveLearn
Dynamical modelling of the elliptical galaxy NGC 2974In this paper we analyse the relations between a previously described oblate Jaffe model for an ellipsoidal galaxy and the observed quantities for NGC 2974, and obtain the length and velocity scales…Zhenglu Jiang·Oct 19, 2008SaveLearn
First performances of the GOLF-NG instrumental prototype observing the Sun in TenerifeThe primary challenge of GOLF-NG (Global Oscillations at Low Frequency New Generation) is the detection of the low-frequency solar gravity and acoustic modes, as well as the possibility to measure…D. Salabert, S. Turck-Chieze, J. C. Barriere et al.·Oct 19, 2008SaveLearn
High Energy Sources Monitored with OMCThe Optical Monitoring Camera on-board INTEGRAL (OMC) provides Johnson V band photometry of any potentially variable source within its field of view. Taking advantage of the INTEGRAL capabilities…D. Risquez, A. Domingo, M. D. Caballero-Garcia et al.·Oct 19, 2008SaveLearn
Long-term multi-frequency monitoring of microquasarsWe discuss the results of the radio studies of the X-ray binaries with relativistic jets. We carried out a multi-frequency (1-30 GHz) daily monitoring of the radio flux variability of the…Sergei A. Trushkin, Nikolaj A. Nizhelskij, Nikolaj N. Bursov·Oct 19, 2008SaveLearn
Kolmogorov stochasticity parameter measuring the randomness in Cosmic Microwave BackgroundThe Kolmogorov stochasticity parameter (KSP) is applied to quantify the degree of randomness (stochasticity) in the temperature maps of the Cosmic Microwave Background radiation maps. It is shown…V. G. Gurzadyan, A. A. Kocharyan·Oct 18, 2008SaveLearn
A model of Hall reconnectionThe rate of quasi-stationary, two-dimensional magnetic reconnection is calculated in the framework of incompressible Hall magnetohydrodynamics (MHD). The calculation is based on the solution of…Leonid M. Malyshkin·Oct 18, 2008SaveLearn
Modeling the Disk (three-phase) Interstellar MediumThe evolution of galactic disks from their early stages is dominated by gasdynamical effects such as gas infall, galactic fountains, and galactic outflows, and further more. The influence of these…Gerhard Hensler·Oct 18, 2008SaveLearn
Reality of Moving Groups in the GalaxyThe existence of old dispersed stellar groups within the Milky Way disk is still controversial. Are they the debris of ancient star-forming aggregates, or short-lived artifacts of dynamical origin?…G. M. De Silva, K. C. Freeman, J. Bland-Hawthorn et al.·Oct 18, 2008SaveLearn
The evolution of a pre-heated Intergalactic MediumWe analyse the evolution of the Intergalactic Medium (IGM) by means of an extended set of large box size hydrodynamical simulations which include pre-heating. We focus on the properties of the z~2…S. Borgani, M. Viel·Oct 18, 2008SaveLearn
Interaction of massive stars with their surroundingsDue to their short lifetimes but their enormous energy release in all stages of their lives massive stars are the major engines for the comic matter circuit. They affect not only their close…Gerhard Hensler·Oct 18, 2008SaveLearn
Multi-Frequency Synthesis of VLBI Images Using a Generalized Maximum Entropy MethodA new multi-frequency synthesis algorithm for reconstructing images from multi-frequency VLBI data is proposed. The algorithm is based on a generalized maximum-entropy method, and makes it possible…Anisa T. Bajkova·Oct 18, 2008SaveLearn
The Dust cloud around the White Dwarf G 29-38. 2. Spectrum from 5-40 microns and mid-infrared variabilityWe model the mineralogy and distribution of dust around the white dwarf G29-39 using the infrared spectrum from 1-35 microns and combining a wide range of materials based on spectral studies of…William T. Reach, Carey Lisse, Ted von Hippel et al.·Oct 18, 2008SaveLearn
The nucleus of NGC 253 and its massive stellar clusters at parsec scalesVery Large Telescope adaptive optics images of NGC 253 with resolutions down to 200 mas resolve the central 300 pc of this galaxy in ~ 37 infrared (IR) bright knots, a factor of 3 larger than…Juan Antonio Fernández-Ontiveros, M. Almudena Prieto, Jose Antonio Acosta-Pulido·Oct 17, 2008SaveLearn
Kinematic Properties and Stellar Populations of Faint Early-Type Galaxies: II. Line-Strength Measurements of Central Coma GalaxiesWe present line-strength measurements for 74 early-type galaxies in the core of the Coma cluster reaching down to velocity dispersions, sigma, of 30 km/s. The index-sigma relations for our sample,…Ana Matkovic, Rafael Guzman, Patricia Sanchez-Blazquez et al.·Oct 17, 2008SaveLearn
Dust Biasing of Damped Lyman Alpha Systems: a Bayesian AnalysisIf damped Lyman alpha systems (DLAs) contain even modest amounts of dust, the ultraviolet luminosity of the background quasar can be severely diminished. When the spectrum is redshifted, this leads…Andrew Pontzen, Max Pettini·Oct 17, 2008SaveLearn
Standing on the shoulders of giants: Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solidsCentimeter and meter sized solid particles in protoplanetary disks are trapped within long lived high pressure regions, creating opportunities for collapse into planetesimals and planetary embryos.…W. Lyra, A. Johansen, H. Klahr et al.·Oct 17, 2008SaveLearn
No observational constraints from hypothetical collisions of hypothetical dark halo primordial black holes with galactic objectsIt was suggested by several authors that hypothetical primordial black holes (PBHs) may contribute to the dark matter in our Galaxy. There are strong constraints based on the Hawking evaporation that…Marek A. Abramowicz, Julia K. Becker, Peter L. Biermann et al.·Oct 17, 2008SaveLearn
Dynamical Study of A1689 from Wide-Field VLT/VIMOS Spectroscopy: Mass Profile, Concentration Parameter, and Velocity AnisotropyWe examine the dynamics structure of the rich cluster A1689, combining VLT/VIMOS spectroscopy with Subaru/Suprime-Cam imaging. The radial velocity distribution of 500 cluster members is…Doron Lemze, Tom Broadhurst, Yoel Rephaeli et al.·Oct 17, 2008SaveLearn
First results from the NEMO Phase 1 experimentThe NEMO prototype detector, called "NEMO Phase-1", has been successfully operated at 2000 m depth from December 2006 to May 2007. The apparatus comprises a Junction Box and a…Isabella Amore·Oct 17, 2008SaveLearn
Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre ArrayAims. We investigate the cosmological evolution of large- and small-scale magnetic fields in galaxies in the light of present models of formation and evolution of galaxies. Methods. We use the dynamo…Tigran G. Arshakian, Rainer Beck, Marita Krause et al.·Oct 17, 2008SaveLearn