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Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA
Ilbert, O.1; McCracken, H. J.2; Le Fevre, O.1; Capak, P.3; Dunlop, J.4; Karim, A.5,6; Renzini, M. A.7; Caputi, K.8; Boissier, S.1; Arnouts, S.9; Aussel, H.10; Comparat, J.1; Guo, Q.11; Hudelot, P.2; Kartaltepe, J.12; Kneib, J. P.1; Krogager, J. K.13; Le Floc'h, E.14; Lilly, S.15; Mellier, Y.2; Milvang-Jensen, B.13; Moutard, T.1; Onodera, M.15; Richard, J.16,17; Salvato, M.18,19; Sanders, D. B.20; Scoville, N.21; Silverman, J. D.22; Taniguchi, Y.23; Tasca, L.1; Thomas, R.1; Toft, S.13; Tresse, L.1; Vergani, D.24; Wolk, M.2; Zirm, A.13
AbstractWe 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 photometric redshifts. By comparing these photometric redshifts with 10,800 spectroscopic redshifts from the zCOSMOS bright and faint surveys, we find a precision of sigma(Delta z/(1+z)) = 0.008 at i(+) < 22.5 and sigma(Delta z/(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 greater than or similar to 10(10.7-10.9) M-circle dot. 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 similar to 3 to z similar to 1, the density of quiescent galaxies increases over the entire mass range. Their comoving stellar mass density increases by 1.6 dex between z similar to 3 and z similar to 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-circle dot 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.
KeywordGalaxies: Distances And Redshifts Galaxies: Evolution Galaxies: Formation Galaxies: Star Formation Galaxies: Stellar Content
Indexed BySCI
WOS IDWOS:000323893500055
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Cited Times:439[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Affiliation1.Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
2.Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France
3.CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA
4.Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland
5.Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England
6.Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany
7.Univ Padua, Dipartimento Astron, I-35122 Padua, Italy
8.Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands
9.Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA
10.Univ Paris 07, AIM Unite Mixte Rech CEA CNRS, Paris, France
11.Chinese Acad Sci, Natl Astron Observ, Partner Grp, Max Planck Inst Astrophys, Beijing 100012, Peoples R China
12.Natl Opt Astron Observ, Tucson, AZ 85719 USA
13.Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark
14.Univ Paris Diderot, CNRS, Lab AIM, F-91190 Gif Sur Yvette, France
15.Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland
16.Univ Lyon 1, CRAL, F-69561 St Genis Laval, France
17.CNRS, UMR 5574, F-69561 St Genis Laval, France
18.Max Planck Inst Extraterr Phys, D-85741 Garching, Germany
19.Excellence Cluster, D-85748 Garching, Germany
20.Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA
21.CALTECH, Pasadena, CA 91125 USA
22.Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan
23.Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan
24.INAF IASFBO, I-40129 Bologna, Italy
Recommended Citation
GB/T 7714
Ilbert, O.,McCracken, H. J.,Le Fevre, O.,et al. Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA[J]. ASTRONOMY & ASTROPHYSICS,2013,556.
APA Ilbert, O..,McCracken, H. J..,Le Fevre, O..,Capak, P..,Dunlop, J..,...&Zirm, A..(2013).Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA.ASTRONOMY & ASTROPHYSICS,556.
MLA Ilbert, O.,et al."Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA".ASTRONOMY & ASTROPHYSICS 556(2013).
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