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Mass assembly and morphological transformations since z ∼ 3 from CANDELS

Huertas-Company, M. and Bernardi, M. and Pérez-González, P. G. and Ashby, M. L. N. and Barro, G. and Conselice, C. and Daddi, E. and Dekel, A. and Dimauro, P. and Faber, S. M. and Grogin, N. A. and Kartaltepe, J. S. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and Mei, S. and Shankar, F. (2016) Mass assembly and morphological transformations since z ∼ 3 from CANDELS. Monthly Notices of the Royal Astronomical Society, 462 (4). pp. 4495-4516. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20161116-110824892

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Abstract

We quantify the evolution of the stellar mass functions (SMFs) of star-forming and quiescent galaxies as a function of morphology from z ∼ 3 to the present. Our sample consists of ∼50 000 galaxies in the CANDELS fields (∼880 arcmin^2), which we divide into four main morphological types, i.e. pure bulge-dominated systems, pure spiral disc-dominated, intermediate two-component bulge+disc systems and irregular disturbed galaxies. At z ∼ 2, 80 per cent of the stellar mass density of star-forming galaxies is in irregular systems. However, by z ∼ 0.5, irregular objects only dominate at stellar masses below 10^9 M_⊙. A majority of the star-forming irregulars present at z ∼ 2 undergo a gradual transformation from disturbed to normal spiral disc morphologies by z ∼ 1 without significant interruption to their star formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects, because the fraction of bulge-dominated star-forming galaxies with M^*/M_⊙ > 10^(10.7) reaches 40 per cent at z < 1. Quenching implies the presence of a bulge: the abundance of massive red discs is negligible at all redshifts over 2 dex in stellar mass. However, the dominant quenching mechanism evolves. At z > 2, the SMF of quiescent galaxies above M* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 < z < 2, the majority of newly quenched galaxies are discs with a significant central bulge. This suggests that mass quenching at this epoch starts from the inner parts and preserves the disc. At z < 1, the high-mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below 10^(10) M_⊙. These low-mass galaxies are compact, bulge-dominated systems, which were environmentally quenched: destruction of the disc through ram-pressure stripping is the likely process.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stw1866DOIArticle
http://mnras.oxfordjournals.org/content/462/4/4495/suppl/DC1PublisherSupporting Information
ORCID:
AuthorORCID
Pérez-González, P. G.0000-0003-4528-5639
Ashby, M. L. N.0000-0002-3993-0745
Barro, G.0000-0001-6813-875X
Conselice, C.0000-0003-1949-7638
Daddi, E.0000-0002-3331-9590
Dekel, A.0000-0003-4174-0374
Faber, S. M.0000-0003-4996-214X
Kartaltepe, J. S.0000-0001-9187-3605
Koekemoer, A. M.0000-0002-6610-2048
Koo, D. C.0000-0003-3385-6799
Mei, S.0000-0002-2849-559X
Additional Information:© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 July 22. Received 2016 July 22; in original form 2016 May 2. First published online July 30, 2016. Thanks to R. Sheth for comments on an early draft. Thanks to the anonymous referee for a constructive and quick report.
Subject Keywords:galaxies: abundances galaxies: evolution galaxies: high-redshift galaxies: structure
Issue or Number:4
Record Number:CaltechAUTHORS:20161116-110824892
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161116-110824892
Official Citation:M. Huertas-Company, M. Bernardi, P. G. Pérez-González, M. L. N. Ashby, G. Barro, C. Conselice, E. Daddi, A. Dekel, P. Dimauro, S. M. Faber, N. A. Grogin, J. S. Kartaltepe, D. D. Kocevski, A. M. Koekemoer, D. C. Koo, S. Mei, and F. Shankar Mass assembly and morphological transformations since z ∼ 3 from CANDELS MNRAS (November 11, 2016) Vol. 462 4495-4516 doi:10.1093/mnras/stw1866 first published online July 30, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72053
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:17 Nov 2016 00:25
Last Modified:09 Mar 2020 13:19

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