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GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 &lt;<i>z</i>&lt; 2 FROM THE S-COSMOS SURVEY

O. IlbertLaboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceM. SalvatoCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125, USAE. Le Floc’hInstitute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, HI 96822, USAH. AusselAIM Unité Mixte de Recherche CEA CNRS, Université Paris VII UMR n158, Paris, FranceP. CapakSpitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USAH. J. McCrackenInstitut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, 98 bis Boulevard Arago, 75014 Paris, FranceB. MobasherDepartment of Physics and Astronomy, University of California, Riverside, CA 92521, USAJ. S. KartaltepeInstitute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, HI 96822, USAN. Z. ScovilleCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125, USAD. B. SandersInstitute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, HI 96822, USAS. ArnoutsCanada France Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USAK. BundyDepartment of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Room 101, Toronto, ON M58 3H4, CanadaP. CassataLaboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceJean‐Paul KneibLaboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceA. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAO. Le FèvreLaboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceS. J. LillyDepartment of Physics, ETH Zurich, CH-8093 Zurich, SwitzerlandJ. SuraceSpitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USAYoshiaki TaniguchiResearch Center for Space and Cosmic Evolution, Ehime University, Bunkyo-cho 2-5, Matsuyama 790-8577, JapanL. TascaDepartment of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Room 101, Toronto, ON M58 3H4, CanadaD. J. ThompsonLBT Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USAL. TresseLaboratoire d'Astrophysique de Marseille, Université de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceMichel ZamojskiCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125, USAG. ZamoraniINAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, ItalyE. ZuccaINAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy
2010en
ABI

Аннотация

We follow the galaxy stellar mass assembly by morphological and spectral type in the COSMOS 2 deg^2 field. We derive the stellar mass functions and stellar mass densities from z = 2 to z = 0.2 using 196,000 galaxies selected at F_(3.6 μm) &gt; 1 μJy with accurate photometric redshifts (σ_[(zphot−zspec)]/(1+zspec) = 0.008 at i^+ &lt; 22.5). Using a spectral classification, we find that z ~ 1 is an epoch of transition in the stellar mass assembly of quiescent galaxies. Their stellar mass density increases by 1.1 dex between z = 1.5-2 and z = 0.8-1 (Δt ~ 2.5 Gyr), but only by 0.3 dex between z = 0.8-1 and z ~ 0.1 (Δt ~ 6 Gyr). Then, we add the morphological information and find that 80%-90% of the massive quiescent galaxies (logM ~ 11) have an elliptical morphology at z &lt; 0.8. Therefore, a dominant mechanism links the shutdown of star formation and the acquisition of an elliptical morphology in massive galaxies. Still, a significant fraction of quiescent galaxies present a Spi/Irr morphology at low mass (40%-60% at logM ~ 9.5), but this fraction is smaller than predicted by semi-analytical models using a "halo quenching" recipe. We also analyze the evolution of star-forming galaxies and split them into "intermediate activity" and "high activity" galaxies. We find that the most massive "high activity" galaxies end their high star formation rate phase first. Finally, the space density of massive star-forming galaxies becomes lower than the space density of massive elliptical galaxies at z &lt; 1. As a consequence, the rate of "wet mergers" involved in the formation of the most massive ellipticals must decline very rapidly at z &lt; 1, which could explain the observed slow down in the assembly of these quiescent and massive sources.

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Идентификаторы

DOI
10.1088/0004-637x/709/2/644

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Цитирований: 1Использованных источников: 0
Показатели — AkademScholar