Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function-Reference-Cited by-同舟云学术

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

Published:2019-06-10 Issue:1 Volume:488 Page:1-17
ISSN:0035-8711
Container-title:Monthly Notices of the Royal Astronomical Society
language:en
Short-container-title:

Author:

Zhang Y¹^ORCID,Miller C J²³,Rooney P⁴,Bermeo A⁴,Romer A K⁴,Vergara Cervantes C⁴,Rykoff E S⁵⁶,Hennig C⁷⁸,Das R³,McKay T³,Song J⁹,Wilcox H¹⁰,Bacon D¹⁰,Bridle S L¹¹,Collins C¹²,Conselice C¹³,Hilton M¹⁴,Hoyle B¹⁵,Kay S¹⁶,Liddle A R¹⁷,Mann R G¹⁸,Mehrtens N¹⁹,Mayers J⁴,Nichol R C¹⁰,Sahlén M²⁰,Stott J²¹,Viana P T P²²²³,Wechsler R H⁵⁶²⁴,Abbott T²⁵,Abdalla F B²⁶²⁷,Allam S¹,Benoit-Lévy A²⁶²⁸²⁹,Brooks D²⁶,Buckley-Geer E¹,Burke D L⁵⁶,Carnero Rosell A³⁰³¹,Carrasco Kind M³²³³,Carretero J³⁴,Castander F J³⁵,Crocce M³⁵,Cunha C E⁵,D’Andrea C B³⁶,da Costa L N³⁰³¹,Diehl H T¹,Dietrich J P⁷⁸,Eifler T F³⁷³⁸,Flaugher B¹,Fosalba P³⁵,García-Bellido J³⁹,Gaztanaga E³⁵,Gerdes D W²³,Gruen D⁵⁶,Gruendl R A³²³³,Gschwend J³⁰³¹,Gutierrez G¹,Honscheid K⁴⁰⁴¹,James D J⁴²,Jeltema T⁴³,Kuehn K⁴⁴,Kuropatkin N¹,Lima M³⁰⁴⁵,Lin H¹,Maia M A G³⁰³¹,March M³⁶,Marshall J L¹⁹,Melchior P⁴⁶,Menanteau F³²³³,Miquel R³⁴⁴⁷,Ogando R L C³⁰³¹,Plazas A A³⁸,Sanchez E⁴⁸,Schubnell M³,Sevilla-Noarbe I⁴⁸,Smith M⁴⁹,Soares-Santos M¹,Sobreira F³⁰⁵⁰,Suchyta E⁵¹,Swanson M E C³³,Tarle G³,Walker A R²⁵,

Affiliation:

1. Fermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USA

2. Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA

3. Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA

4. Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton BN1 9QH, UK

5. Kavli Institute for Particle Astrophysics & Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, USA

6. SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA

7. Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr 1, D-81679 Munich, Germany

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

9. Taejon Christian International School, Yuseong, Daejeon 34035, South Korea

10. Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK

11. Jodrell Bank Center for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK

12. Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK

13. School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD, UK

14. Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZuluNatal, Westville Campus, Durban 4000, South Africa

15. Fakultät für Physik, Universitäts-Sternwarte, Ludwig-Maximilians Universität München, Scheinerstr 1, D-81679 München, Germany

16. Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK

17. Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK

18. Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

19. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA

20. Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden

21. Physics Department, Lancaster University, Lancaster LA1 4YB, UK

22. Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, P-4150-762 Porto, Portugal

23. Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre 687, P-4169-007 Porto, Portugal

24. Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA

25. Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile

26. Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK

27. Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown 6140, South Africa

28. CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014 Paris, France

29. Institut d’Astrophysique de Paris, Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, F-75014 Paris, France

30. Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil

31. Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil

32. Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA

33. National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA

34. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain

35. Institute of Space Sciences, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain

36. Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA

37. Department of Physics, California Institute of Technology, Pasadena, CA 91125, USA

38. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA

39. Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain

40. Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA

41. Department of Physics, The Ohio State University, Columbus, OH 43210, USA

42. Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195, USA

43. Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA

44. Australian Astronomical Observatory, North Ryde, NSW 2113, Australia

45. Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP 05314-970, Brazil

46. Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA

47. Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain

48. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain

49. School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK

50. Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859 Campinas, SP, Brazil

51. Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA

Abstract

Abstract Using ∼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 ($13.5 \le \rm {log_{10}}(M_{200crit}) \sim \lt 15.0$). 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 (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m* with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ${\sim } 20{{\ \rm per\ cent}}$ 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.

Funder

U.S. Department of Energy

National Science Foundation

Science and Technology Facilities Council

Higher Education Funding Council for England

University of Illinois

University of Chicago

Ohio State University

Conselho Nacional de Desenvolvimento Científico e Tecnológico

Ministério da Ciência, Tecnologia e Inovação

Deutsche Forschungsgemeinschaft

Argonne National Laboratory