Mass assembly in quiescent and star-forming galaxies since z similar or equal to 4 from UltraVISTA

O. Ilbert*, H. J. McCracken, O. Le Fevre, 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. MellierB. Milvang-Jensen, T. Moutard, M. Onodera, J. Richard, M. Salvato, D. B. Sanders, N. Scoville, J. D. Silverman, Y. Taniguchi, L. Tasca, Rajat Thomas, S. Toft, L. Tresse, D. Vergani, M. Wolk, A. Zirm

*Corresponding author for this work

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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 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.

Original languageEnglish
Article numberA55
Number of pages19
JournalAstronomy & astrophysics
Volume556
DOIs
Publication statusPublished - Aug-2013

Keywords

  • galaxies: distances and redshifts
  • galaxies: evolution
  • galaxies: formation
  • galaxies: star formation
  • galaxies: stellar content
  • ACTIVE GALACTIC NUCLEI
  • VLT DEEP SURVEY
  • SPECTRAL ENERGY-DISTRIBUTIONS
  • STELLAR POPULATION SYNTHESIS
  • FORMATION HISTORY
  • COSMOS FIELD
  • RED SEQUENCE
  • LUMINOSITY FUNCTION
  • PHOTOMETRIC REDSHIFTS
  • KECK SPECTROSCOPY
  • Multi-color photometry of star-forming galaxies

    Ilbert, O. (Contributor), McCracken, H. J. (Contributor), Le Fèvre, O. (Contributor), Capak, P. (Contributor), Dunlop, J. (Contributor), Karim, A. (Contributor), Renzini, M. A. (Contributor), Caputi, K. (Contributor), Boissier, S. (Contributor), Arnouts, S. (Contributor), Aussel, H. (Contributor), Comparat, J. (Contributor), Guo, Q. (Contributor), Hudelot, P. (Contributor), Kartaltepe, J. (Contributor), Kneib, J. P. (Contributor), Krogager, J. K. (Contributor), Le Floc'h, E. (Contributor), Lilly, S. (Contributor), Mellier, Y. (Contributor), Milvang-Jensen, B. (Contributor), Moutard, T. (Contributor), Onodera, M. (Contributor), Richard, J. (Contributor), Salvato, M. (Contributor), Sanders, D. B. (Contributor), Scoville, N. (Contributor), Silverman, J. D. (Contributor), Taniguchi, Y. (Contributor), Tasca, L. (Contributor), Thomas, R. (Contributor), Toft, S. (Contributor), Tresse, L. (Contributor), Vergani, D. (Contributor), Wolk, M. (Contributor) & Zirm, A. (Contributor), University of Groningen, 25-Jul-2013

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