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The stellar mass function of quiescent galaxies in 2 &amp;lt; <i>z</i> &amp;lt; 2.5 protoclusters

Adit H EdwardDepartment of Physics and Astronomy, University of Waterloo , Waterloo, Ontario N2L 3G1 , CanadaMichael L. BaloghDepartment of Physics and Astronomy, University of Waterloo , Waterloo, Ontario N2L 3G1 , CanadaYannick M BahéInstitute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL) , Observatoire de Sauverny, CH-1290 Versoix , SwitzerlandMichael C. CooperDepartment of Physics and Astronomy, University of California , Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697 , USAN. A. HatchSchool of Physics and Astronomy, University of Nottingham , Nottingham NG7 2RD , UKJustin MarchioniDepartment of Physics and Astronomy, University of Waterloo , Waterloo, Ontario N2L 3G1 , CanadaAdam MuzzinDepartment of Physics and Astronomy, York University , 4700, Keele Street, Toronto, Ontario MJ3 1P3 , CanadaAllison NobleSchool of Earth and Space Exploration, Arizona State University , Tempe, AZ 85287 , USAGregory RudnickDepartment of Physics and Astronomy, University of Kansas , Lawrence, KS 66045 , USABenedetta VulcaniINAF – Osservatorio Astronomico di Padova , Vicolo Osservatorio 5, I-35122 Padova , ItalyGillian WilsonDepartment of Physics, University of California Merced 5200 Lake Road , Merced, CA 95343 , USAG. De LuciaINAF – Astronomical Observatory of Trieste , via G.B. Tiepolo 11, I-34143 Trieste , ItalyR. DemarcoDepartamento de Astronomía, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción , Casilla 160-C, Concepción , ChileBen ForrestDepartment of Physics and Astronomy, University of California Davis , One Shields Avenue, Davis, CA 95616 , USAMichaela HirschmannInstitute for Physics, Laboratory for Galaxy Evolution and Spectral modelling, Ecole Polytechnique Federale de Lausanne , Observatoire de Sauverny, Chemin Pegasi 51, CH-1290 Versoix , SwitzerlandG. CastignaniDipartimento di Fisica e Astronomia ‘Augusto Righi, Alma Mater Studiorum Universitá di Bologna , Via Gobetti 93/2, I-40129 Bologna , ItalyPierluigi CeruloDepartamento de Ingeniería Informática y Ciencias de la Computaciíon, Facultad de Ingeniería, Universidad de Concepción , Casilla 160-C, Concepción , ChileRose FinnDepartment of Physics and Astronomy, Siena College , 515 Loudon Rd, Loudonville, NY 12211 , USAGuillaume HewittDepartment of Physics and Astronomy, University of Waterloo , Waterloo, Ontario N2L 3G1 , CanadaP. JablonkaGEPI, Observatoire de Paris, Université PSL , CNRS, Place Jules Janssen, F-92190 Meudon , FranceTadayuki KodamaAstronomical Institute, Tohoku University , 6-3, Aramaki, Aoba, Sendai, Miyagi 980-8578 , JapanSophie MaurogordatoObservatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, Université Côte d’Azur , CS 34229, F-06304 Nice Cedex 4 , FranceJulie NantaisInstituto de Astrofísica, Departamento de Ciencias Físicas, Universidad Andres Bello , Fernandez Concha 700, Las Condes 7591538, Santiago, Región Metropolitana , ChileLizhi XieTianjin Astrophysics Center, Tianjin Normal University , Binshuixidao 393, 300387 Tianjin , People’s Republic of China
2023en
ABI

Аннотация

ABSTRACT We present an analysis of the galaxy stellar mass function (SMF) of 14 known protoclusters between 2.0 &amp;lt; z &amp;lt; 2.5 in the COSMOS field, down to a mass limit of 109.5 M⊙. We use existing photometric redshifts with a statistical background subtraction, and consider star-forming and quiescent galaxies identified from (NUV − r) and (r − J) colours separately. Our fiducial sample includes galaxies within 1 Mpc of the cluster centres. The shape of the protocluster SMF of star-forming galaxies is indistinguishable from that of the general field at this redshift. Quiescent galaxies, however, show a flatter SMF than in the field, with an upturn at low mass, though this is only significant at ∼2σ. There is no strong evidence for a dominant population of quiescent galaxies at any mass, with a fraction &amp;lt;15 per cent at 1σ confidence for galaxies with log M*/M⊙ &amp;lt; 10.5. We compare our results with a sample of galaxy groups at 1 &amp;lt; z &amp;lt; 1.5, and demonstrate that a significant amount of environmental quenching must take place between these epochs, increasing the relative abundance of high-mass ($\rm M_{\ast } \gt 10^{10.5} {\rm M}_{\odot }$) quiescent galaxies by a factor ≳ 2. However, we find that at lower masses ($\rm M_{\ast } \lt 10^{10.5} {\rm M}_{\odot }$), no additional environmental quenching is required.

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DOI
10.1093/mnras/stad3751

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