The GALFA-HI Survey: TechniquesWe explain the entire process by which we conduct the Galactic Arecibo L-Band Feed Array HI (GALFA-HI) survey. The survey is a high resolution (3.4'), large area (13000 deg2), large Galactic…J. E. G. Peek, Carl Heiles·Oct 7, 2008SaveLearn
Thermodynamics of atmospheric circulation on hot JupitersAtmospheric circulation on tidally-locked exoplanets is driven by the absorption and reradiation of heat from the host star. They are natural heat engines, converting heat into mechanical energy. A…J. Goodman·Oct 7, 2008SaveLearn
The Enrichment of the Intracluster MediumTo determine the relative contributions of galactic and intracluster stars to the enrichment of the intracluster medium (ICM), we present X-ray surface brightness, temperature, and Fe abundance…Suresh Sivanandam, Ann I. Zabludoff, Dennis Zaritsky et al.·Oct 7, 2008SaveLearn
The Motion of Water Masers in the Pre-Planetary Nebula IRAS 16342-3814We present high angular resolution observations, using the Very Long Baseline Array (VLBA) of the NRAO, of the high-velocity water masers toward the "water-fountain" pre-planetary nebula,…M. J Claussen, R. Sahai, M. R. Morris·Oct 7, 2008SaveLearn
Automated LASCO CME catalog for solar cycle 23: are CMEs scale invariant?In this paper we present the first automatically constructed LASCO CME catalog, a result of the application of the Computer Aided CME Tracking software (CACTus) on the LASCO archive during the…E. Robbrecht, D. Berghmans, R. A. M. Van der Linden·Oct 7, 2008SaveLearn
A Fallback Disk Accretion-Involved Formation Channel to PSR J1903+0327The discovery of the eccentric binary and millisecond pulsar PSR J1903+03273 has raised interesting questions about the formation mechanisms of this peculiar system. Here we present a born-fast…Xi-Wei Liu, Xiang-Dong Li·Oct 7, 2008SaveLearn
A Comprehensive X-ray Spectral Analysis of the Seyfert 1.5 NGC 3227We present results of a 100 ks XMM observation of the Seyfert 1.5 NGC 3227. Our best-fit broadband model to the pn spectrum consists of a moderately flat (photon index 1.57) hard X-ray power-law…A. Markowitz, J. N. Reeves, I. M. George et al.·Oct 7, 2008SaveLearn
The cluster-galaxy cross-spectrum: an additional probe of cosmological and halo parametersThere are several wide field galaxy and cluster surveys planned for the nearest future, e.g. BOSS, WFMOS, ADEPT, Hetdex, SPT, eROSITA. In the simplest approach one would analyze these independently,…Gert Huetsi, Ofer Lahav·Oct 7, 2008SaveLearn
Fabry-Perot Absorption Line Spectroscopy of the Galactic Bar. I. KinematicsWe use Fabry-Perot absorption line imaging spectroscopy to measure radial velocities using the Ca II 8542 line in 3360 stars towards three lines of sight in the Milky Way's bar: Baade's…Naseem Rangwala, T. B. Williams, K. Z. Stanek·Oct 7, 2008SaveLearn
Physical Properties of Very Powerful FRII Radio GalaxiesWe estimate ages and physical properties of powerful radio galaxies. An analysis of new multi-wavelength VLA observations of eleven very powerful classical double (FRIIb) radio galaxies with…Christopher P. O'Dea, Ruth A. Daly, Preeti Kharb et al.·Oct 7, 2008SaveLearn
On the distance and reddening of the starburst galaxy IC10We present deep and accurate optical photometry of the Local Group starburst galaxy IC10. The photometry is based on two sets of images collected with the Advanced Camera for Surveys and with the…N. Sanna, G. Bono, P. B. Stetson et al.·Oct 7, 2008SaveLearn
Redshifted emission lines and radiative recombination continuum from the Wolf-Rayet binary theta Muscae: evidence for a triplet system?We present XMM-Newton observations of the WC binary Theta Muscae (WR 48), the second brightest Wolf-Rayet binary in optical wavelengths. The system consists of a short-period (19.1375 days) WC5/WC6 +…Yasuharu Sugawara, Yohko Tsuboi, Yoshitomo Maeda·Oct 7, 2008SaveLearn
Dynamical evolution and spectral characteristics of the stellar group Mamajek 2The dynamical evolution of the recently detected stellar group Mamajek 2 is studied by means of its past 3D orbit. The past orbits of the open clusters NGC 2516 and α Persei, belonging to the…E. Jilinski, V. G. Ortega, R. de la Reza et al.·Oct 7, 2008SaveLearn
Stellar spindown: From the ONC to the SunRotation is a key parameter in the evolution of stars. From 1 Myr (the age of the ONC) to 4.5 Gyr (the age of the Sun), solar-like stars lose about 1-2 orders of specific angular momentum. The main…Alexander Scholz·Oct 7, 2008SaveLearn
Multiple flaring activity in the supergiant fast X-ray transient IGR J08408-4503 observed with SwiftIGR J08408-4503 is a supergiant fast X-ray transient discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194. We report on the analysis of two outbursts caught by…P. Romano, L. Sidoli, G. Cusumano et al.·Oct 7, 2008SaveLearn
Investigation of astrophysical phenomena in short time scales with "Pi of the Sky" apparatusIn this thesis the data analysis designed by author for the "Pi of the Sky" experiment is presented. The data analysis consists of data reduction and specific algorithms for identification of…Marcin Sokolowski·Oct 7, 2008SaveLearn
Photometric/spectroscopic analyses and magnetic activity in young late-type starsWe present the work in progress of a study based on photometric and spectroscopic observations of young Weak-line T Tauri and Post T Tauri stars just attiving on the Zero Age Main Sequence. This…K. Biazzo, A. Frasca, E. Marilli et al.·Oct 7, 2008SaveLearn
Multiwavelength spectral and high time resolution observations of SWIFT J1753.5-0127: new activity?We have conducted an extensive observational campaign of SWIFT J1753.5-0127 during June 2007 after its bright outburst episode in 2005. We have performed multi-band optical photometry, optical…M. Durant, P. Gandhi, T. Shahbaz et al.·Oct 7, 2008SaveLearn
A 42.3-43.6 GHz spectral survey of Orion BN/KL: First detection of the v=0 J=1-0 line from the isotopologues 29SiO and 30SiOWe have surveyed molecular line emission from Orion BN/KL from 42.3 to 43.6 GHz with the Green Bank Telescope. Sixty-seven lines were identified and ascribed to 13 different molecular species. The…C. Goddi, L. J. Greenhill, E. M. L. Humphreys et al.·Oct 7, 2008SaveLearn
Ionization Quenching Factor Measurement of Helium 4The ionization quenching factor (IQF) is defined as the fraction of energy released by a recoil in a medium through ionization compared with its total kinetic energy. At low energies, in the range of…D. Santos, F. Mayet, O. Guillaudin et al.·Oct 7, 2008SaveLearn
Interstellar Plasma Turbulence Spectrum Toward the Pulsars PSR B0809+74 and B0950+08Interstellar scintillations of pulsars PSR B0809+74 and B0950+08 have been studied using observations at low frequencies (41, 62, 89, and 112 MHz). Characteristic temporal and frequency scales of…T. V. Smirnova, V. I. Shishov·Oct 7, 2008SaveLearn
Starburst triggered by compressive tides in galaxy mergersThe tidal field of galaxies is known generally to be disruptive. However, in the case of galaxy mergers, a compressive mode of tidal wave may develop and last long enough to cocoon the formation of…Florent Renaud, Christian Theis, Christian M. Boily·Oct 7, 2008SaveLearn
Vanishing hardness-flux correlation in Cygnus X-1: signs of the disc moving outAims. We investigate observations of the X-ray binary Cygnus X-1 with unusually high hardness and low flux. In particular, we study the characteristic frequencies seen in the PDS and the…M. Axelsson, L. Hjalmarsdotter, L. Borgonovo et al.·Oct 7, 2008SaveLearn
Mass Supply to Galactic Center due to Nested Bars in the GalaxyWe investigate rapid mass supply process by nested bars in the Galaxy by numerical simulation. We simulate gas flow in the whole galaxy disk with nested bars, which are the outer bar and the inner…Daisuke Namekata, Asao Habe, Hidenori Matsui et al.·Oct 7, 2008SaveLearn
A microlensing study of the accretion disc in the quasar MG 0414+0534Observations of gravitational microlensing in multiply imaged quasars currently provide the only direct probe of quasar emission region structure on sub-microarcsecond scales. Analyses of…N. F. Bate, D. J. E. Floyd, R. L. Webster et al.·Oct 7, 2008SaveLearn