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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

Lee, Bomee and Giavalisco, Mauro and Whitaker, Katherine and Williams, Christina C. and Ferguson, Henry C. and Acquaviva, Viviana and Koekemoer, Anton M. and Straughn, Amber N. and Guo, Yicheng and Kartaltepe, Jeyhan S. and Lotz, Jennifer and Pacifici, Camilla and Croton, Darren J. and Somerville, Rachel S. and Lu, Yu (2018) 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. Astrophysical Journal, 853 (2). Art. No. 131. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20180201-112824988

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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 Σ_1 (the projected density within the central 1 kpc), while younger, star-forming galaxies span a much broader range of Σ_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 Σ_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 Σ_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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aaa40fDOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aaa40f/metaPublisherArticle
https://arxiv.org/abs/1706.02311arXivDiscussion Paper
ORCID:
AuthorORCID
Lee, Bomee0000-0003-1954-5046
Giavalisco, Mauro0000-0002-7831-8751
Whitaker, Katherine0000-0001-7160-3632
Williams, Christina C.0000-0003-2919-7495
Ferguson, Henry C.0000-0001-7113-2738
Acquaviva, Viviana0000-0002-6788-6315
Koekemoer, Anton M.0000-0002-6610-2048
Guo, Yicheng0000-0003-2775-2002
Kartaltepe, Jeyhan S.0000-0001-9187-3605
Lotz, Jennifer0000-0003-3130-5643
Pacifici, Camilla0000-0003-4196-0617
Croton, Darren J.0000-0002-5009-512X
Lu, Yu0000-0003-2691-1622
Additional Information:© 2018. The American Astronomical Society. Received 2017 June 5; revised 2017 December 19; accepted 2017 December 21; published 2018 January 31. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. K.E.W. gratefully acknowledge support by NASA through Hubble Fellowship grant No. HF2-51368, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA. R.S.S. acknowledges the generous support of the Downsbrough family.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS5-26555
NASA Hubble FellowshipHF2-51368
NASA Postdoctoral ProgramUNSPECIFIED
Downsbrough familyUNSPECIFIED
Subject Keywords:galaxies: evolution; galaxies: formation; Galaxy: structure; techniques: photometric
Issue or Number:2
Record Number:CaltechAUTHORS:20180201-112824988
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180201-112824988
Official Citation:Bomee Lee et al 2018 ApJ 853 131
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:84626
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:01 Feb 2018 21:40
Last Modified:03 Oct 2019 19:20

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