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Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA

Ilbert, O. and Capak, P. and Scoville, N. (2013) Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA. Astronomy and Astrophysics, 556 . Art. No. A55. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20131004-111419268

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Abstract

We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2 < z < 4. We construct a large, deep (K_s < 24) sample of 220 000 galaxies selected using the new UltraVISTA DR1 data release. Our analysis is based on precise 30-band photometricredshifts. By comparing these photometric redshifts with 10,800 spectroscopic redshifts from the zCOSMOS bright and faint surveys, we find a precision of σ_(Δz/(1 + z)) = 0.008 at i+ < 22.5 and σ_(Δz/(1 + z)) = 0.03 at 1.5 < z < 4. We derive the stellar mass function and correct for the Eddington bias. We find a mass-dependent evolution of the global and star-forming populations, with the low-mass end of the mass functions evolving more rapidly than the high-mass end. This mass-dependent evolution is a direct consequence of the star formation being “quenched” in galaxies more massive than ℳ ≳ 1010.7 − 10.9ℳ_⊙. For the mass function of the quiescent galaxies, we do not find any significant evolution of the high-mass end at z < 1; however we observe a clear flattening of the faint-end slope. From z ~ 3 to z ~ 1, the density of quiescent galaxies increases over the entire mass range. Their comoving stellar mass density increases by 1.6 dex between z ~ 3 and z ~ 1 and by less than 0.2 dex at z < 1. We infer the star formation history from the mass density evolution. This inferred star formation history is in excellent agreement with instantaneous star formation rate measurements at z < 1.5, while we find differences of 0.2 dex at z > 1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 10^(10−10.5)ℳ_⊙ galaxies increases continuously in the redshift range 1 < z < 4. Finally, we compare our results with a semi-analytical model and find that these models overestimate the density of low mass quiescent galaxies by an order of magnitude, while the density of low-mass star-forming galaxies is successfully reproduced.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201321100DOIArticle
http://www.aanda.org/articles/aa/abs/2013/08/aa21100-13/aa21100-13.htmlPublisherArticle
http://arxiv.org/abs/1301.3157arXivDiscussion Paper
Additional Information:© 2013 ESO. Article published by EDP Sciences. Received 14 January 2013. Accepted 30 May 2013. Published online 25 July 2013. We are grateful to the referee for a careful reading of the manuscript and useful suggestions. The authors thank M. Kajisawa, L. Pozzetti, P. Pérez-González and P. Santini for providing their estimates of the mass function. We also thanks P. Behroozi for his useful suggestions. The authors thank J. Donley for providing her catalogue of IRAC power-laws. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. The HST COSMOS program was supported through NASA grant HST-GO-09822. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. H.J. McCracken acknowledges support from the “Programme national cosmologie et galaxies”. J.S.D. acknowledges the support of the European Research Council through an Advanced grant, and the support of the Royal Society via a Wolfson Research Merit Award. S. Toft acknowledges support from the Lundbeck foundation. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This paper is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based in part on archival SEDS data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Dark Cosmology Centre is funded by the Danish National Research Foundation. B.M.J. acknowledges support from the ERC-StG grant EGGS-278202. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
Group:COSMOS
Funders:
Funding AgencyGrant Number
NASAHST-GO-09822
Programme National Cosmologie et GalaxiesUNSPECIFIED
European Research Council Advanced GrantUNSPECIFIED
Royal Society Wolfson Research Merit awardUNSPECIFIED
Lundbeck FoundationUNSPECIFIED
Danish National Research FoundationUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
ERC-StGEGGS-278202
Subject Keywords:galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: star formation; galaxies: stellar content
Record Number:CaltechAUTHORS:20131004-111419268
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20131004-111419268
Official Citation:Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA O. Ilbert, H. J. McCracken, O. Le Fèvre, P. Capak, J. Dunlop, A. Karim, M. A. Renzini, K. Caputi, S. Boissier, S. Arnouts, H. Aussel, J. Comparat, Q. Guo, P. Hudelot, J. Kartaltepe, J. P. Kneib, J. K. Krogager, E. Le Floc’h, S. Lilly, Y. Mellier, B. Milvang-Jensen, T. Moutard, M. Onodera, J. Richard, M. Salvato, D. B. Sanders, N. Scoville, J. D. Silverman, Y. Taniguchi, L. Tasca, R. Thomas, S. Toft, L. Tresse, D. Vergani, M. Wolk and A. Zirm A&A 556 A55 (2013) DOI: http://dx.doi.org/10.1051/0004-6361/201321100
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:41684
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:07 Oct 2013 16:24
Last Modified:06 Jul 2015 17:36

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