THE EVOLUTION OF STAR FORMATION HISTORIES OF QUIESCENT GALAXIES
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Author
Pacifici, Camilla
Kassin, Susan A. Weiner, Benjamin Holden, Bradford Ferguson, Henry C. Koo, David C. Primack, Joel R. Bell, Eric F. Dekel, Avishai Gawiser, Eric Giavalisco, Mauro Rafelski, Marc Simons, Raymond C. Barro, Guillermo Croton, Darren J. Davé, Romeel Fontana, Adriano Grogin, Norman A. Koekemoer, A. Lee, Seong-Kook Salmon, Brett
Affiliation
Univ Arizona, Steward ObservIssue Date
2016-11-18Metadata
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IOP PUBLISHING LTDCitation
THE EVOLUTION OF STAR FORMATION HISTORIES OF QUIESCENT GALAXIES 2016, 832 (1):79 The Astrophysical JournalJournal
The Astrophysical JournalRights
© 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
1538-4357Version
Final published versionSponsors
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.4b4fff7a1775de4750163473a802b086Scopus Count
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