We study the effects of environment on the evolution of galaxies, with an emphasis on two different approaches towards the definition of environment: (1) environment defined based on the local surface density of galaxies and (2) environment defined based on the major components of the cosmic web; i.e., filaments, clusters and the field. In the first approach, surface density field is estimated using a variety of estimators and tested with simulations. Using the estimated surface densities assigned to galaxies, we observe a strong environmental dependence on the properties of galaxies (e.g., SFR, sSFR and the quiescent fraction) at z ≤ 1. We explore the fractional role of stellar mass and environment in quenching the star-formation. In the second approach, we use the Multi-scale Morphology Filter algorithm to disentangle the density field into its component. We apply this method to a sample of star-forming galaxies for a large-scale structure at z ∼0.84 in the HiZELS-COSMOS field. We show that the observed median SFR, stellar mass, sSFR, the mean SFR$-$mass relation and its scatter for star-forming galaxies do not strongly depend on the cosmic web. However, the fraction of H[Alpha] star-forming galaxies varies with environment and is enhanced in filaments. Furthermore, we study the physical properties of a spectroscopic sample of star-forming galaxies in a large filament in the COSMOS field at z ∼0.53, with spectroscopic data taken with the Keck/DEIMOS spectrograph, and compare them with a control sample of field galaxies. We spectroscopically confirm the presence of a large galaxy filament (∼ 8 Mpc). We show that within the uncertainties, the ionization parameter, EW, EW versus sSFR relation, EW versus stellar mass relation, line-of-sight velocity dispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar for filament and field star-forming galaxies. However, we show that on average, filament star-forming galaxies are more metal-enriched (∼ 0.1-0.15 dex) and the electron densities are significantly lower (a factor of ∼17) in filament star-forming systems compared to those in the field. Our results highlight the potential role of galaxy filaments and intermediate-density environments on the evolution of galaxies, which has been poorly investigated.
14.1 Adapted from J. Bennett , M. Donahue , N. Schneider , and M. Voit , Cosmic Perspectives , 2nd ed . ( Reading , Mass .: Addison - Wesley , 2002 ) , p . 629 . 14.2 Adapted from N. F. Comins and W. J. Kaufman III , Discovering the ...
The Carnegie Atlas of Galaxies
美国学者集团、台湾启思文化事业有限公司授权出版
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Galactic Astronomy: Structure and Kinematics
Aimed at a wide-ranging audience including amateur astronomers, science historians, researchers, Hubble Space Telescope (HST) aficionados and students interested in science, this book recounts the progression of events that led to the deep ...
This volume describes the properties and facts about stars and galaxies.
Universe: The Solar System With Starry Night Enthusiast
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Climb Aboard! Explore different types of galaxies! Learn how galaxies are formed! Meet key astronomers examine the tools they use such as the Hubble Space Telescope, satellites, and probes! See an infographic showing Earth in the Milky Way!