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How do galaxies such as our Milky Way come into existence? How do they grow and change over time? The science behind galaxy formation has long been a puzzle, but a University of Arizona-led team of sc...
We present robust statistical estimates of the accuracy of early-type galaxy stellar masses derived from spectral energy distribution (SED) fitting as functions of various empirical and theoretical as...
Star formation in the extended gaseous disk of the isolated galaxy CIG 96     extended  gaseous disk  isolated  galaxy  CIG 96       font style='font-size:12px;'> 2011/9/27
We study the Kennicutt-Schmidt star formation law and efficiency in the gaseous disk of the isolated galaxy CIG 96 (NGC 864), with special emphasis on its unusually large atomic gas (HI) disk (r_HI/r_...
We analyze the dependence of galaxy structure (size and Sersic index) and mode of star formation (\Sigma_SFR and SFR_IR/SFR_UV) on the position of galaxies in the SFR versus Mass diagram. Our sample c...
Nuclear to host galaxy relation of high redshift quasars     Nuclear  redshift quasars  host galaxy       font style='font-size:12px;'> 2009/7/9
Nuclear to host galaxy relation of high redshift quasars。
Big game hunting in the andromeda galaxy:identifying And weighing black holes in low mass x-ray binaries。
An x-ray view of interacting binaries outside the galaxy      x-ray view  galaxy  interacting binaries        font style='font-size:12px;'> 2009/6/17
An x-ray view of interacting binaries outside the galaxy
The detection of supergalactic winds:The edge-on starburst galaxy NGC 4631。
N-Body Simulations of Small Galaxy Groups (Parte A)     N-Body Simulations  Small Galaxy Groups       font style='font-size:12px;'> 2009/6/11
N-Body Simulations of Small Galaxy Groups (Parte A)。
Iso spectroscopy of ultracompact H II regions:element abundance gradient in the galaxy
In this work, based on the analytical model with delayed production approximation developed by Pagel & Tautvaiˇsien˙e (1995) for the Galaxy, the analytic solutions of the distribution of neutron e...

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