TY - JOUR
T1 - The GOGREEN Survey
T2 - A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching
AU - Van Der Burg, Remco F.J.
AU - Rudnick, Gregory
AU - Balogh, Michael L.
AU - Muzzin, Adam
AU - Lidman, Chris
AU - Old, Lyndsay J.
AU - Shipley, Heath
AU - Gilbank, David
AU - McGee, Sean
AU - Biviano, Andrea
AU - Cerulo, Pierluigi
AU - Chan, Jeffrey C.C.
AU - Cooper, Michael
AU - De Lucia, Gabriella
AU - Demarco, Ricardo
AU - Forrest, Ben
AU - Gwyn, Stephen
AU - Jablonka, Pascale
AU - Kukstas, Egidijus
AU - Marchesini, Danilo
AU - Nantais, Julie
AU - Noble, Allison
AU - Pintos-Castro, Irene
AU - Poggianti, Bianca
AU - Reeves, Andrew M.M.
AU - Stefanon, Mauro
AU - Vulcani, Benedetta
AU - Webb, Kristi
AU - Wilson, Gillian
AU - Yee, Howard
AU - Zaritsky, Dennis
N1 - Funding Information:
Acknowledgements. We thank the anonymous reviewer for useful comments that helped to improve and clarify the message of this work. It is a pleasure to thank Ian McCarthy and Allison Man for insightful discussions. We thank Sean Fillingham, Callum Bellhouse, Melinda Townsend and Nicole Drakos for help with the observations. RvdB thanks George Lansbury and Marianne Heida for kindly providing a computer screen that allowed him to efficiently work remotely. We thank the International Space Science Institute (ISSI) for providing financial support and a meeting facility that inspired insightful discussions for team “COSWEB: The Cosmic Web and Galaxy Evolution”. G.R. acknowledges support from the National Science Foundation grants AST-1517815, AST-1716690, and AST-1814159 and NASA HST grant AR-14310. G.R. also acknowledges the support of an ESO visiting science fellowship. R.D. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. The European Space Agency (ESA) Research Fellowship (LJO). Universidad Andrés Bello Internal Project #DI-12-19/R (JN). P.C. acknowledges the support of the ALMA-CONICYT grant no 31180051. This work is supported by the National Science Foundation through grant AST-1517863, by HST program number GO-15294, and by grant number 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). Support for program number GO-15294 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work was supported in part by NSF grants AST-1815475 and AST-1518257. Additional support was provided by NASA through grant AR-14289 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 769130). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 833824). BV acknowledges financial contribution from the grant PRIN MIUR 2017 n.20173ML3WW_001 (PI Cimatti) and from the INAF main-stream funding programme (PI Vulcani). Based on observations obtained at the Gemini Observatory (GS LP-1 and GN LP-4), which is operated by the Association of Universities for Research in Astronomy, Inc., under
Funding Information:
a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 097.A-0734(A) and 097.A-0734(B). Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Based on observations obtained with WIRCam, a joint project of CFHT, the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) in Taiwan, the Korea Astronomy and Space Science Institute (KASI) in Korea, Canada, France, and the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/) supported by the Spanish MINECO through grant AYA2017-84089.
Publisher Copyright:
© ESO 2020.
PY - 2020/6/1
Y1 - 2020/6/1
N2 - 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.
AB - 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.
KW - Galaxies: clusters: general
KW - Galaxies: evolution
KW - Galaxies: luminosity function
KW - Galaxies: photometry
KW - Galaxies: stellar content
KW - Mass function
UR - http://www.scopus.com/inward/record.url?scp=85087915595&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202037754
DO - 10.1051/0004-6361/202037754
M3 - Article
AN - SCOPUS:85087915595
SN - 0004-6361
VL - 638
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A112
ER -