Reversal or no reversal: The evolution of the star formation rate-density relation up to z ~ 1.6

F. Ziparo, P. Popesso, A. Finoguenov, A. Biviano, S. Wuyts, D. Wilman, M. Salvato, M. Tanaka, K. Nandra, D. Lutz, D. Elbaz, M. Dickinson, B. Altieri, H. Aussel, S. Berta, A. Cimatti, D. Fadda, R. Genzel, E. Le Floc'h, B. MagnelliR. Nordon, A. Poglitsch, F. Pozzi, M. Sanchez Portal, L. Tacconi, F. E. Bauer, W. N. Brandt, N. Cappelluti, M. C. Cooper, J. S. Mulchaey

Research output: Contribution to journalArticlepeer-review

32 Scopus citations

Abstract

We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.

Original languageEnglish (US)
Article numberstt1901
Pages (from-to)458-474
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Volume437
Issue number1
DOIs
StatePublished - 2014

Keywords

  • Galaxies: evolution
  • Galaxies: groups: general
  • Galaxies: star formation
  • Infrared: galaxies

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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