The stellar mass function of quiescent galaxies in 2 < z < 2.5 protoclusters

被引：0

作者：

Edward, Adit H. ^{[1
,2
]}

Balogh, Michael L. ^{[1
,2
]}

Bahe, Yannick M. ^{[3
,4
]}

Cooper, M. C. ^{[5
]}

Hatch, Nina A. ^{[6
]}

Marchioni, Justin ^{[1
,2
]}

Muzzin, Adam ^{[4
,7
]}

Noble, Allison ^{[8
]}

Rudnick, Gregory H. ^{[9
]}

Vulcani, Benedetta ^{[10
]}

Wilson, Gillian ^{[11
]}

De Lucia, Gabriella ^{[12
]}

Demarco, Ricardo ^{[13
]}

Forrest, Ben ^{[14
]}

Hirschmann, Michaela ^{[15
]}

Castignani, Gianluca ^{[16
,17
]}

Cerulo, Pierluigi ^{[18
]}

Finn, Rose A. ^{[19
]}

Hewitt, Guillaume ^{[1
,2
]}

Jablonka, Pascale ^{[20
,21
]}

Kodama, Tadayuki ^{[22
]}

Maurogordato, Sophie ^{[23
]}

Nantais, Julie ^{[24
]}

Xie, Lizhi ^{[25
]}

机构：

[1] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[2] Univ Waterloo, Waterloo Ctr Astrophys, Waterloo, ON N2L 3G1, Canada

[3] Ecole Polytech Fed Lausanne EPFL, Inst Phys, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland

[4] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[5] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA

[6] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[7] York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON MJ3 1P3, Canada

[8] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[9] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

[10] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[11] Univ Calif Merced, Dept Phys, 5200 Lake Rd, Merced, CA 95343 USA

[12] INAF Astron Observ Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[13] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Astron, Casilla 160-C, Concepcion, Chile

[14] Univ Calif Davis, Dept Phys & Astron, One Shields Ave, Davis, CA 95616 USA

[15] Ecole Polytech Fed Lausanne, Lab Galaxy Evolut & Spectral Modelling, Observ Sauverny, Inst Phys, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[16] Univ Bologna, Dipartimento Fis & Astron Augusto Righi, Alma Mater Studiorum, Via Gobetti 93-2, I-40129 Bologna, Italy

[17] INAF Osservatorio Astrofis & Sci Spazio Bologna, Via Gobetti 93-3, I-40129 Bologna, Italy

[18] Univ Concepcion, Fac Ingn, Dept Ingn Informat & Ciencias Computaci, Casilla 160-C, Concepcion, Chile

[19] Siena Coll, Dept Phys & Astron, 515 Loudon Rd, Loudonville, NY 12211 USA

[20] Ecole Polytech Fed Lausanne EPFL, Lab Astrophys, CH-1290 Lausanne, Switzerland

[21] Univ PSL, Observ Paris, CNRS, GEPI, Pl Jules Janssen, F-92190 Meudon, France

[22] Tohoku Univ, Astron Inst, 6-3 Aramaki, Sendai, Miyagi 9808578, Japan

[23] Univ Cote dAzur, CNRS, Observ Cote dAzur, Lab Lagrange, Bd Observ CS 34229, F-06304 Nice 4, France

[24] Univ Andres Bello, Dept Ciencias Fis, Inst Astrofis, Fernandez Concha 700, Santiago 7591538, Region Metropol, Chile

[25] Tianjin Normal Univ, Tianjin Astrophys Ctr, Binshuixidao 393, Tianjin 300387, Peoples R China

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 527卷 / 03期

基金：

美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

galaxies: clusters: general; galaxies: evolution; SIMILAR-TO; 1; OPTICAL LUMINOSITY DENSITY; STAR-FORMATION RATES; RED SEQUENCE; SPECTROSCOPIC CONFIRMATION; CLUSTER GALAXIES; DARK-MATTER; SYSTEMATIC SEARCH; PASSIVE GALAXIES; PROTO-CLUSTER;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of the galaxy stellar mass function (SMF) of 14 known protoclusters between 2.0 < z < 2.5 in the COSMOS field, down to a mass limit of 10(9.5) M-circle dot. 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 similar to 2 sigma. There is no strong evidence for a dominant population of quiescent galaxies at any mass, with a fraction <15 per cent at 1 sigma confidence for galaxies with log M-*/M-circle dot < 10.5. We compare our results with a sample of galaxy groups at 1 < z < 1.5, and demonstrate that a significant amount of environmental quenching must take place between these epochs, increasing the relative abundance of high-mass (M-& lowast; > 10(10.5)M(circle dot)) quiescent galaxies by a factor greater than or similar to 2. However, we find that at lower masses (M-& lowast; < 10(10.5)M circle dot), no additional environmental quenching is required.

引用

页码：8598 / 8617

页数：20

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The stellar mass function of quiescent galaxies in 2 &lt; z &lt; 2.5 protoclusters

The stellar mass function of quiescent galaxies in 2 < z < 2.5 protoclusters