Issues in joint SZ and optical cluster findingWe apply simple optical and SZ cluster finders to mock galaxy catalogues and SZ flux maps created from dark matter halos in a (1 Gpc/h)3 dark matter simulation, at redshifts 0.5 and 0.9. At each…J. D. Cohn, Martin White·Sep 1, 2008SaveLearn
Modelling radiation damage to ESA's Gaia satellite CCDsThe Gaia satellite is a high-precision astrometry, photometry and spectroscopic ESA cornerstone mission, currently scheduled for launch in late 2011. Its primary science drivers are the composition,…G. M. Seabroke, A. D. Holland, M. S. Cropper·Sep 1, 2008SaveLearn
Dependence of S-Process Nucleosynthesis in Massive Stars on Triple-Alpha and 12C(a,g)16O Reaction Rate UncertaintiesWe have studied the sensitivity of s-process nucleosynthesis in massive stars to +/- 2 sigma variations in the rates of the triple alpha and 12C(a,g)16O reactions. We simulated the evolution of…Clarisse Tur, Alexander Heger, Sam M. Austin·Sep 1, 2008SaveLearn
Theoretical modeling of propagation of magneto-acoustic waves in magnetic regions below sunspotsWe use 2D numerical simulations and eikonal approximation, to study properties of MHD waves traveling below the solar surface through the magnetic structure of sunspots. We consider a series of…E. Khomenko, A. Kosovichev, M. Collados et al.·Sep 1, 2008SaveLearn
Phantom dark energy and cosmological solutions without the Big Bang singularityThe hypothesis is rapidly gaining popularity that the dark energy pervading our universe is extra-repulsive (-p>ρ). The density of such a substance(usually called phantom energy) grows with the…Anton Baushev·Sep 1, 2008SaveLearn
Using SPICA Space Telescope to characterize ExoplanetsWe present the 3.5m SPICA space telescope, a proposed Japanese-led JAXA-ESA mission scheduled for launch around 2017. The actively cooled (<5 K), single aperture telescope and monolithic mirror will…J. R. Goicoechea, B. Swinyard, G. Tinetti et al.·Sep 1, 2008SaveLearn
VLT detection of a red supergiant progenitor of the type IIP supernova 2008bkWe report the identification of a source coincident with the position of the nearby type II-P supernova (SN) 2008bk in high quality optical and near-infrared pre-explosion images from the ESO Very…S. Mattila, S. J. Smartt, J. J. Eldridge et al.·Sep 1, 2008SaveLearn
The modulation of SiO maser polarization by Jovian planetsSearching for planets in the atmosphere of AGB stars is difficult, due to confusion with the stellar wind and pulsations. The aim here is to provide a complementary strategy for planet search in such…Helmut Wiesemeyer·Sep 1, 2008SaveLearn
The Evolution of Galaxy Disks in Dense Environments - Lessons from Compact Galaxy GroupsDisk galaxies in compact galaxy groups exhibit a remarkable shortfall of neutral hydrogen compared to both isolated spirals and spirals in more loose groups, but the origin of this HI deficiency…J. Rasmussen, T. J. Ponman, L. Verdes-Montenegro et al.·Sep 1, 2008SaveLearn
AAOmega radial velocities rule out current membership of the planetary nebula NGC 2438 in the open cluster M46We present new radial velocity measurements of 586 stars in a one-degree field centered on the open cluster M46, and the planetary nebula NGC 2438 located within a nuclear radius of the cluster. The…L. L. Kiss, Gy. M. Szabo, Z. Balog et al.·Sep 1, 2008SaveLearn
Atomic diffusion and mixing in old stars II. Observations of stars in the globular cluster NGC 6397 with VLT/FLAMES-GIRAFFEEvolutionary trends in the surface abundances of heavier elements have recently been identified in the globular cluster NGC 6397 ([Fe/H]=-2), indicating the operation of atomic diffusion in these…K. Lind, A. J. Korn, P. S. Barklem et al.·Sep 1, 2008SaveLearn
[NeII] emission line profiles from photoevaporative disc windsI model profiles of the [NeII] forbidden emission line at 12.81um, emitted by photoevaporative winds from discs around young, solar-mass stars. The predicted line luminosities (~ 1E-6 Lsun) are…R. D. Alexander·Sep 1, 2008SaveLearn
Proper Motions of Thermal Radio Sources near HH 7-11 in the NGC 1333 Star Forming RegionStar forming regions are expected to show linear proper motions due to the relative motion of the Sun with respect to the region. These proper motions appear superposed to the proper motions expected…C. Carrasco-Gonzalez, G. Anglada, L. F. Rodriguez et al.·Sep 1, 2008SaveLearn
The Deep SWIRE Field I. 20cm Continuum Radio Observations: A Crowded SkyWe present results from deep radio observations taken with the VLA at a center frequency of 1400 MHz cover a region of the SWIRE Spitzer Legacy survey, centered at 10 46 00, 59 01 00 (J2000). The…Frazer N. Owen, Glenn E. Morrison·Sep 1, 2008SaveLearn
A Derivation of the Luminosity Function of the Kuiper Belt from a Broken Power-Law Size DistributionWe have derived a model of the Kuiper belt luminosity function exhibited by a broken power-law size distribution. This model allows direct comparison of the observed luminosity function to the…W. C. Fraser, JJ. Kavelaars·Sep 1, 2008SaveLearn
AGN Host Galaxy Morphologies in COSMOSWe use HST/ACS images and a photometric catalog of the COSMOS field to analyze morphologies of the host galaxies of approximately 400 AGN candidates at redshifts 0.3 < z < 1.0. We compare the AGN…J. M. Gabor, C. D. Impey, K. Jahnke et al.·Sep 1, 2008SaveLearn
The photometric evolution of star clusters and the preferential loss of low-mass bodies - with an application to globular clustersTo obtain an accurate description of broad-band photometric star cluster evolution, certain effects should be accounted for, such as the preferential loss of low-mass stars and the retain of stellar…J. M. Diederik Kruijssen, Henny J. G. L. M. Lamers·Sep 1, 2008SaveLearn
Millimeter interferometry of W3 IRS5: A Trapezium in the makingAlthough most young massive stars appear to be part of multiple systems, it is poorly understood how this multiplicity influences the formation of massive stars. The high-mass star-forming region W3…J. A. Rodón, H. Beuther, T. Megeath et al.·Sep 1, 2008SaveLearn
A Bayesian approach to power-spectrum significance estimation, with application to solar neutrino dataThe usual procedure for estimating the significance of a peak in a power spectrum is to calculate the probability of obtaining that value or a larger value by chance, on the assumption that the time…P. A. Sturrock·Sep 1, 2008SaveLearn
Large-scale magnetic topologies of early M dwarfsWe present here additional results of a spectropolarimetric survey of a small sample of stars ranging from spectral type M0 to M8 aimed at investigating observationally how dynamo processes operate…JF Donati, J Morin, P Petit et al.·Sep 1, 2008SaveLearn
Systematic uncertainties in MonteCarlo simulations of the atmospheric muon flux in the 5-line ANTARES detectorThe ANTARES detector was operated in a configuration with 5 lines for a period of 10 months from February until November 2007. The duty cycle was better than 80% during this period and almost 2*10**7…A. Margiotta·Sep 1, 2008SaveLearn
A large stellar evolution database for population synthesis studies. IV. Integrated properties and spectraThis paper is the 4th in a series describing the latest additions to the BaSTI stellar evolution database, which consists of a large set of homogeneous models and tools for population synthesis…Susan M. Percival, Maurizio Salaris, Santi Cassisi et al.·Sep 1, 2008SaveLearn
The effect of gas-dynamics on semi-analytic modeling of cluster galaxiesWe study the degree to which non-radiative gas dynamics affects the merger histories of haloes along with subsequent predictions from a semi-analytic model (SAM) of galaxy formation. To this aim, we…A. Saro, G. De Lucia, K. Dolag et al.·Sep 1, 2008SaveLearn
A broad-band spectral analysis of eight radio loud type 1 AGN selected in the hard X-ray bandStarting from a complete sample of type I AGN observed by INTEGRAL in the 20-40 keV band, we have selected a set of 8 AGN which can be classified as radio loud objects according to their 1.4 GHz…M. Molina, L. Bassani, A. Malizia et al.·Sep 1, 2008SaveLearn
Fields from a relativistic magnetic explosionFollowing Prendergast we study the relativistically expanding electromagnetic fields generated by an axisymmetric explosion of magnetic energy in a small volume. The magnetic field expands uniformly…K. N. Gourgouliatos, D. Lynden-Bell·Sep 1, 2008SaveLearn