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    The Intrinsic Characteristics of Galaxies on the SFR–M ∗ Plane at 1.2 < z < 4: I. The Correlation between Stellar Age, Central Density, and Position Relative to the Main Sequence

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    Author
    Lee, Bomee cc
    Giavalisco, Mauro cc
    Whitaker, Katherine E. cc
    Williams, Christina C. cc
    Ferguson, Henry C. cc
    Acquaviva, Viviana cc
    Koekemoer, A. cc
    Straughn, Amber N.
    Guo, Yicheng cc
    Kartaltepe, Jeyhan S. cc
    Lotz, Jennifer cc
    Pacifici, Camilla cc
    Croton, Darren J. cc
    Somerville, Rachel S.
    Lu, Yu cc
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2018-01-31
    Keywords
    galaxies: evolution
    galaxies: formation
    Galaxy: structure
    techniques: photometric
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    The Intrinsic Characteristics of Galaxies on the SFR–M ∗ Plane at 1.2 < z < 4: I. The Correlation between Stellar Age, Central Density, and Position Relative to the Main Sequence 2018, 853 (2):131 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2018. 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 use the deep CANDELS observations in the GOODS North and South fields to revisit the correlations between stellar mass (M-*), star formation rate (SFR) and morphology, and to introduce a fourth dimension, the mass-weighted stellar age, in galaxies at 1.2 < z < 4. We do this by making new measures of M-*, SFR, and stellar age thanks to an improved SED fitting procedure that allows various star formation history for each galaxy. Like others, we find that the slope of the main sequence (MS) of star formation in the (M-*; SFR) plane bends at high mass. We observe clear morphological differences among galaxies across the MS, which also correlate with stellar age. At all redshifts, galaxies that are quenching or quenched, and thus old, have high Sigma(1) (the projected density within the central 1 kpc), while younger, star-forming galaxies span a much broader range of Sigma(1), which includes the high values observed for quenched galaxies, but also extends to much lower values. As galaxies age and quench, the stellar age and the dispersion of Sigma(1) for fixed values of M* shows two different regimes: one at the low-mass end, where quenching might be driven by causes external to the galaxies; the other at the high-mass end, where quenching is driven by internal causes, very likely the mass given the low scatter of Sigma(1) (mass quenching). We suggest that the monotonic increase of central density as galaxies grow is one manifestation of a more general phenomenon of structural transformation that galaxies undergo as they evolve.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aaa40f
    Version
    Final published version
    Sponsors
    NASA [NAS5-26555]; NASA through Hubble Fellowship grant - Space Telescope Science Institute [HF2-51368]; Downsbrough family
    Additional Links
    http://stacks.iop.org/0004-637X/853/i=2/a=131?key=crossref.f963f08365dfd45585994b52b62fcf1b
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aaa40f
    Scopus Count
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    UA Faculty Publications

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