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Title: THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 {<=} z {<=} 2.2

Abstract

We study the buildup of the bimodal galaxy population using the NEWFIRM Medium-Band Survey, which provides excellent redshifts and well-sampled spectral energy distributions of {approx}27, 000 galaxies with K < 22.8 at 0.4 < z < 2.2. We first show that star-forming galaxies and quiescent galaxies can be robustly separated with a two-color criterion over this entire redshift range. We then study the evolution of the number density and mass density of quiescent and star-forming galaxies, extending the results of the COMBO-17, DEEP2, and other surveys to z = 2.2. The mass density of quiescent galaxies with M {approx}> 3 x 10{sup 10} M{sub sun} increases by a factor of {approx}10 from z {approx} 2 to the present day, whereas the mass density in star-forming galaxies is flat or decreases over the same time period. Modest mass growth by a factor of {approx}2 of individual quiescent galaxies can explain roughly half of the strong density evolution at masses >10{sup 11} M{sub sun}, due to the steepness of the exponential tail of the mass function. The rest of the density evolution of massive, quiescent galaxies is likely due to transformation (e.g., quenching) of the massive star-forming population, a conclusion which ismore » consistent with the density evolution we observe for the star-forming galaxies themselves, which is flat or decreasing with cosmic time. Modest mass growth does not explain the evolution of less massive quiescent galaxies ({approx}10{sup 10.5} M{sub sun}), which show a similarly steep increase in their number densities. The less massive quiescent galaxies are therefore continuously formed by transforming galaxies from the star-forming population.« less

Authors:
 [1]; ; ; ;  [2];  [3];  [4];  [5]; ; ;  [6];  [7]
  1. European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago (Chile)
  2. Department of Astronomy, Yale University, New Haven, CT 06520 (United States)
  3. Department of Physics and Astronomy, Tufts University, Medford, MA 02155 (United States)
  4. Leiden Observatory, P.O. Box 9513, NL-2300 RA Leiden (Netherlands)
  5. Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States)
  6. Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101 (United States)
  7. Department of Physics and Astronomy, University of Kansas, Malott Hall, Room 1082, 1251 Wescoe Hall Drive, Lawrence, KS 66045 (United States)
Publication Date:
OSTI Identifier:
21587526
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 739; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/739/1/24; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DENSITY; ENERGY SPECTRA; GALACTIC EVOLUTION; GALAXIES; MASS; RED SHIFT; STARS; EVOLUTION; PHYSICAL PROPERTIES; SPECTRA

Citation Formats

Brammer, Gabriel B., Whitaker, K. E., Van Dokkum, P. G., Lee, K.-S., Muzzin, A., Marchesini, D., Franx, M., Kriek, M., Labbe, I., Quadri, R. F., Williams, R., and Rudnick, G., E-mail: gbrammer@eso.org. THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 {<=} z {<=} 2.2. United States: N. p., 2011. Web. doi:10.1088/0004-637X/739/1/24; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Brammer, Gabriel B., Whitaker, K. E., Van Dokkum, P. G., Lee, K.-S., Muzzin, A., Marchesini, D., Franx, M., Kriek, M., Labbe, I., Quadri, R. F., Williams, R., & Rudnick, G., E-mail: gbrammer@eso.org. THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 {<=} z {<=} 2.2. United States. doi:10.1088/0004-637X/739/1/24; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Brammer, Gabriel B., Whitaker, K. E., Van Dokkum, P. G., Lee, K.-S., Muzzin, A., Marchesini, D., Franx, M., Kriek, M., Labbe, I., Quadri, R. F., Williams, R., and Rudnick, G., E-mail: gbrammer@eso.org. Tue . "THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 {<=} z {<=} 2.2". United States. doi:10.1088/0004-637X/739/1/24; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
@article{osti_21587526,
title = {THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 {<=} z {<=} 2.2},
author = {Brammer, Gabriel B. and Whitaker, K. E. and Van Dokkum, P. G. and Lee, K.-S. and Muzzin, A. and Marchesini, D. and Franx, M. and Kriek, M. and Labbe, I. and Quadri, R. F. and Williams, R. and Rudnick, G., E-mail: gbrammer@eso.org},
abstractNote = {We study the buildup of the bimodal galaxy population using the NEWFIRM Medium-Band Survey, which provides excellent redshifts and well-sampled spectral energy distributions of {approx}27, 000 galaxies with K < 22.8 at 0.4 < z < 2.2. We first show that star-forming galaxies and quiescent galaxies can be robustly separated with a two-color criterion over this entire redshift range. We then study the evolution of the number density and mass density of quiescent and star-forming galaxies, extending the results of the COMBO-17, DEEP2, and other surveys to z = 2.2. The mass density of quiescent galaxies with M {approx}> 3 x 10{sup 10} M{sub sun} increases by a factor of {approx}10 from z {approx} 2 to the present day, whereas the mass density in star-forming galaxies is flat or decreases over the same time period. Modest mass growth by a factor of {approx}2 of individual quiescent galaxies can explain roughly half of the strong density evolution at masses >10{sup 11} M{sub sun}, due to the steepness of the exponential tail of the mass function. The rest of the density evolution of massive, quiescent galaxies is likely due to transformation (e.g., quenching) of the massive star-forming population, a conclusion which is consistent with the density evolution we observe for the star-forming galaxies themselves, which is flat or decreasing with cosmic time. Modest mass growth does not explain the evolution of less massive quiescent galaxies ({approx}10{sup 10.5} M{sub sun}), which show a similarly steep increase in their number densities. The less massive quiescent galaxies are therefore continuously formed by transforming galaxies from the star-forming population.},
doi = {10.1088/0004-637X/739/1/24; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 739,
place = {United States},
year = {2011},
month = {9}
}