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    THE EVOLUTION OF STAR FORMATION HISTORIES OF QUIESCENT GALAXIES

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    Pacifici_2016_ApJ_832_79.pdf
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    Author
    Pacifici, Camilla cc
    Kassin, Susan A. cc
    Weiner, Benjamin cc
    Holden, Bradford cc
    Gardner, Jonathan P.
    Faber, Sandra M.
    Ferguson, Henry C. cc
    Koo, David C. cc
    Primack, Joel R. cc
    Bell, Eric F. cc
    Dekel, Avishai cc
    Gawiser, Eric cc
    Giavalisco, Mauro cc
    Rafelski, Marc cc
    Simons, Raymond C. cc
    Barro, Guillermo cc
    Croton, Darren J. cc
    Davé, Romeel cc
    Fontana, Adriano cc
    Grogin, Norman A. cc
    Koekemoer, A. cc
    Lee, Seong-Kook cc
    Salmon, Brett cc
    Somerville, Rachel
    Behroozi, Peter
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2016-11-18
    Keywords
    galaxies: evolution
    galaxies: formation
    galaxies: statistics
    galaxies: stellar content
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    THE EVOLUTION OF STAR FORMATION HISTORIES OF QUIESCENT GALAXIES 2016, 832 (1):79 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2016. 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
    Although there has been much progress in understanding how galaxies evolve, we still do not understand how and when they stop forming stars and become quiescent. We address this by applying our galaxy spectral energy distribution models, which incorporate physically motivated star formation histories (SFHs) from cosmological simulations, to a sample of quiescent galaxies at 0.2 < z < 2.1. A total of 845 quiescent galaxies with multi-band photometry spanning rest-frame ultraviolet through near-infrared wavelengths are selected from the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) data set. We compute median SFHs of these galaxies in bins of stellar mass and redshift. At all redshifts and stellar masses, the median SFHs rise, reach a peak, and then decline to reach quiescence. At high redshift, we find that the rise and decline are fast, as expected, because the universe is young. At low redshift, the duration of these phases depends strongly on stellar mass. Low-mass galaxies (log(M*/M-circle dot) similar to 9.5) grow on average slowly, take a long time to reach their peak of star formation (greater than or similar to 4 Gyr), and then the declining phase is fast (less than or similar to 2 Gyr). Conversely, high-mass galaxies (log(M*/M-circle dot) similar to 11) grow on average fast (less than or similar to 2 Gyr), and, after reaching their peak, decrease the star formation slowly (greater than or similar to 3). These findings are consistent with galaxy stellar mass being a driving factor in determining how evolved galaxies are, with high-mass galaxies being the most evolved at any time (i.e., downsizing). The different durations we observe in the declining phases also suggest that low- and high-mass galaxies experience different quenching mechanisms, which operate on different timescales.
    ISSN
    1538-4357
    DOI
    10.3847/0004-637X/832/1/79
    Version
    Final published version
    Sponsors
    NASA [NAS5-26555]; SAK through HST Grant [AR-12828.001]; Director's Discretionary Research Fund (DDRF)
    Additional Links
    http://stacks.iop.org/0004-637X/832/i=1/a=79?key=crossref.4b4fff7a1775de4750163473a802b086
    ae974a485f413a2113503eed53cd6c53
    10.3847/0004-637X/832/1/79
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    UA Faculty Publications

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