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    z ∼ 2: An Epoch of Disk Assembly

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    Simons_2017_ApJ_843_46.pdf
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    Author
    Simons, Raymond C. cc
    Kassin, Susan A. cc
    Weiner, Benjamin cc
    Faber, Sandra M.
    Trump, Jonathan R. cc
    Heckman, Timothy M. cc
    Koo, David C. cc
    Pacifici, Camilla cc
    Primack, Joel R. cc
    Snyder, Gregory F. cc
    Vega, Alexander de la cc
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2017-06-30
    Keywords
    galaxies: evolution
    galaxies: kinematics and dynamics
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    z ∼ 2: An Epoch of Disk Assembly 2017, 843 (1):46 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2017. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star formation at z similar to 2 to today. Measurements of galaxy rotation velocity V-rot, which quantify ordered motions, and gas velocity dispersion sigma(g), which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift over 0.1 < z < 2.5, spanning 10 Gyr. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported (V-rot > sigma(g)). By z = 2, 50% and 70% of galaxies are rotationally supported at low (10(9)-10(10) M-circle dot) and high (10(10)-10(11) M-circle dot) stellar mass, respectively. For V-rot > 3 sigma(g), the percentage drops below 35% for all masses. From z = 2 to now, galaxies exhibit remarkably smooth kinematic evolution on average. All galaxies tend toward rotational support with time, and higher-mass systems reach it earlier. This is largely due to a mass-independent decline in sigma(g) by a factor of 3 since z - 2. Over the same time period, V-rot increases by a factor of 1.5 in low-mass systems but does not evolve at high mass. These trends in V-rot and sigma(g) are at a fixed stellar mass and therefore should not be interpreted as evolutionary tracks for galaxy populations. When populations are linked in time via abundance matching, sigma(g) declines as before and V-rot strongly increases with time for all galaxy populations, enhancing the evolution in V-rot sigma(g). These results indicate that z = 2 is a period of disk assembly, during which strong rotational support is only just beginning to emerge.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aa740c
    Version
    Final published version
    Sponsors
    Space Telescope Science Institute; NASA [NAS 5-26555]; NSF [AST-0808133]; STScI
    Additional Links
    http://stacks.iop.org/0004-637X/843/i=1/a=46?key=crossref.6ec900336d72e7249c02b70a17e4c053
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aa740c
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    UA Faculty Publications

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