Galaxies in X-ray selected clusters and groups in Dark Energy Survey data - II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

被引：9

作者：

Zhang, Y. ^{[1
]}

Miller, C. J. ^{[2
,3
]}

Rooney, P. ^{[4
]}

Bermeo, A. ^{[4
]}

Romer, A. K. ^{[4
]}

Cervantes, C. Vergara ^{[4
]}

Rykoff, E. S. ^{[5
,6
]}

Hennig, C. ^{[7
,8
]}

Das, R. ^{[3
]}

Mckay, T. ^{[3
]}

Song, J. ^{[9
]}

Wilcox, H. ^{[10
]}

Bacon, D. ^{[10
]}

Bridle, S. L. ^{[11
]}

Collins, C. ^{[12
]}

Conselice, C. ^{[13
]}

Hilton, M. ^{[14
]}

Hoyle, B. ^{[15
]}

Kay, S. ^{[11
]}

Liddle, A. R. ^{[16
]}

Mann, R. G. ^{[17
]}

Mehrtens, N. ^{[18
,19
]}

Mayers, J. ^{[4
]}

Nichol, R. C. ^{[10
]}

Sahlen, M. ^{[20
]}

Stott, J. ^{[21
]}

Viana, P. T. P. ^{[22
,23
]}

Wechsler, R. H. ^{[5
,6
,24
]}

Abbott, T. ^{[25
]}

Abdalla, F. B. ^{[26
,27
]}

Allam, S. ^{[1
]}

Benoit-Levy, A. ^{[26
,28
,29
]}

Brooks, D. ^{[26
]}

Buckley-Geer, E. ^{[1
]}

Burke, D. L. ^{[5
,6
]}

Carnero Rosell, A. ^{[30
,31
]}

Kind, M. Carrasco ^{[32
,33
]}

Carretero, J. ^{[34
]}

Castander, F. J. ^{[35
]}

Crocce, M. ^{[35
]}

Cunha, C. E. ^{[5
]}

D'Andrea, C. B. ^{[36
]}

da Costa, L. N. ^{[30
,31
]}

Diehl, H. T. ^{[1
]}

Dietrich, J. P. ^{[7
,8
]}

Eifler, T. F. ^{[37
,38
]}

Flaugher, B. ^{[1
]}

Fosalba, P. ^{[35
]}

Garcia-Bellido, J. ^{[39
]}

Gaztanaga, E. ^{[35
]}

机构：

[1] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[2] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[3] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[4] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

[5] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[6] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[7] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[8] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany

[9] Taejon Christian Int Sch, Yuseong 34035, Daejeon, South Korea

[10] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[11] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England

[12] Liverpool John Moores Univ, Astrophys Res Inst, IC2 Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

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

[14] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, Westville Campus, ZA-4000 Durban, South Africa

[15] Ludwig Maximilians Univ Munchen, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

[16] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[17] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[18] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[19] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[20] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden

[21] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England

[22] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Porto, Portugal

[23] Univ Porto, Dept Fis & Astron, Fac Ciencias, Rua Campo Alegre 687, P-4169007 Porto, Portugal

[24] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[25] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[26] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[27] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

[28] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[29] UPMC Univ Paris 06, Inst Astrophys Paris, Sorbonne Univ, UMR 7095, F-75014 Paris, France

[30] LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[31] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[32] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[33] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[34] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[35] CSIC, IEEC, Inst Space Sci, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[36] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[37] CALTECH, Dept Phys, Pasadena, CA 91125 USA

[38] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[39] Univ Autonoma Madrid, Inst Fis Teor, CSIC, E-28049 Madrid, Spain

[40] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[41] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[42] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA

[43] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[44] Australian Astron Observ, N Ryde, NSW 2113, Australia

[45] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

[46] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[47] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

[48] CIEMAT, E-28040 Madrid, Spain

[49] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[50] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 488卷 / 01期

基金：

美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会; 澳大利亚研究理事会;

关键词：

galaxies: clusters: general; galaxies: evolution; COLOR-MAGNITUDE RELATION; STELLAR POPULATION SYNTHESIS; HALO OCCUPATION DISTRIBUTION; STAR-FORMATION; MORPHOLOGICAL EVOLUTION; SKY SURVEY; MASS; PHOTOMETRY; ORIGIN; MATTER;

D O I：

10.1093/mnras/stz1612

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using similar to 100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function ( LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift ( 0.1 < z < 1.05) and cluster mass ( 13.5 <= log(10)( M-200crit) similar to< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break ( m*) to a faint end power-law slope ( alpha). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (similar to 1.9 sigma) evolution in the faint end slope alpha versus redshift. We also find no dependence in alpha or m* with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to similar to 20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.

引用

页码：1 / 17

页数：17

共 28 条

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