The GOGREEN Survey: a deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching

Research output: Contribution to journalArticlepeer-review


  • Remco F. J. van der Burg
  • Gregory Rudnick
  • Michael L. Balogh
  • Adam Muzzin
  • Chris Lidman
  • Lyndsay J. Old
  • Heath Shipley
  • David Gilbank
  • Andrea Biviano
  • Pierluigi Cerulo
  • Jeffrey C. C. Chan
  • Michael Cooper
  • Gabriella De Lucia
  • Ricardo Demarco
  • Ben Forrest
  • Stephen Gwyn
  • Pascale Jablonka
  • Egidijus Kukstas
  • Danilo Marchesini
  • Julie Nantais
  • Allison Noble
  • Irene Pintos-Castro
  • Bianca Poggianti
  • Andrew M. M. Reeves
  • Mauro Stefanon
  • Benedetta Vulcani
  • Kristi Webb
  • Gillian Wilson
  • Howard Yee
  • Dennis Zaritsky

Colleges, School and Institutes


We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 < z < 1.4 drawn from the Gemini Observations of Galaxies in Rich Early ENvironments (GOGREEN) survey. Based on more than 500 h of Gemini/GMOS spectroscopy and deep multi-band photometry taken with a range of observatories, we probe the SMFs down to a stellar mass limit of 109.7 M (109.5 M for star-forming galaxies). At this early epoch, the fraction of quiescent galaxies is already highly elevated in the clusters compared to the field at the same redshift. The quenched fraction excess (QFE) represents the fraction of galaxies that would be star-forming in the field but are quenched due to their environment. The QFE is strongly mass dependent, and increases from ∼30% at M = 109.7 M to ∼80% at M = 1011.0 M. Nonetheless, the shapes of the SMFs of the two individual galaxy types, star-forming and quiescent galaxies, are identical between cluster and field to high statistical precision. Nevertheless, along with the different quiescent fractions, the total galaxy SMF is also environmentally dependent, with a relative deficit of low-mass galaxies in the clusters. These results are in stark contrast with findings in the local Universe, and therefore require a substantially different quenching mode to operate at early times. We discuss these results in light of several popular quenching models.

Bibliographic note

19 pages, 9 figures (excluding appendices). Accepted for publication in A&A


Original languageEnglish
Article numberA112
Number of pages23
JournalAstronomy and Astrophysics
Publication statusPublished - 23 Jun 2020


  • astro-ph.GA, galaxies: luminosity function, mass function, alaxies: stellar content, galaxies: clusters: general, galaxies: evolution, galaxies: photometry