THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 [< or =, slant] z < 0.8 IN THE DEEP2/AEGIS SURVEY

The shutdown of star formation in galaxies is generally termed "quenching." This paper addresses quenching by searching for traces of possible quenching processes through their effects on galaxy structural parameters such as stellar mass (M sub(*)), M sub(*)/r sub(e), surface stellar mass...

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Bibliographic Details
Published in:The Astrophysical journal 2012-12, Vol.760 (2), p.1-25
Main Authors: Cheung, Edmond, Faber, S M, Koo, David C, Dutton, Aaron A, Simard, Luc, McGrath, Elizabeth J, Huang, J-S, Bell, Eric F, Dekel, Avishai, Fang, Jerome J
Format: Article
Language:English
Subjects:
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
AXIAL SYMMETRY
COLOR
Construction
CORRELATIONS
DENSITY
GALACTIC EVOLUTION
GALAXIES
GALAXY NUCLEI
INDEXES
MASS
Mathematical models
NONLUMINOUS MATTER
QUENCHING
RED SHIFT
Searching
SHOCK HEATING
STAR EVOLUTION
STARS
Stellar mass
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Summary:The shutdown of star formation in galaxies is generally termed "quenching." This paper addresses quenching by searching for traces of possible quenching processes through their effects on galaxy structural parameters such as stellar mass (M sub(*)), M sub(*)/r sub(e), surface stellar mass density (~M sub(*)/r super(2) sub(e)), and Sersic index (n). We analyze the rest-frame U-B color correlations versus these structural parameters using a sample of galaxies in the redshift range 0.5 [< or =, slant] z < 0.8 from the DEEP2/AEGIS survey. We assess the tightness of the color relationships by measuring their "overlap regions," defined as the area in color-parameter space in which red and blue galaxies overlap; the parameter that minimizes these overlap regions is considered to be the most effective color discriminator. We discuss a two-stage model for quenching in which galaxy star formation rates are controlled by their dark halos while they are still in the blue cloud and a second quenching process sets in later, associated with the central stellar mass buildup.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/760/2/131