CODEX weak lensing mass catalogue and implications on the mass–richness relation

Author:

Kiiveri K12,Gruen D34ORCID,Finoguenov A1ORCID,Erben T5,van Waerbeke L6,Rykoff E34,Miller L7,Hagstotz S8,Dupke R9101112,Patrick Henry J13,Kneib J-P1415,Gozaliasl G12ORCID,Kirkpatrick C C12ORCID,Cibirka N1617,Clerc N18ORCID,Costanzi M19,Cypriano E S16,Rozo E20,Shan H21,Spinelli P22,Valiviita J223,Weller J1724

Affiliation:

1. Department of Physics, University of Helsinki, PO Box 64, FI-00014 Helsinki, Finland

2. Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, PO Box 64, FI-00014, Helsinki, Finland

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

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

5. Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany

6. Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural road, Vancouver BC V6T 1Z1, Canada

7. Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK

8. Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova University Centre, SE 106 91 Stockholm, Sweden

9. Observatório Nacional, Rua Gal. José Cristino, Rio de Janeiro 20921-400, Brasil

10. Department of Astronomy, University of Michigan, 311 West Hall 1085 South University Ave. Ann Arbor, MI 48109, USA

11. Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487, USA

12. Eureka Scientific Inc., 2452 Delmer St Suite 100, Oakland, CA 94602, USA

13. Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA

14. Laboratoire d’Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland

15. Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388 Marseille, France

16. Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, R. do Matão 1226, 05508-090 São Paulo, Brasil

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

18. CNRS, IRAP, 9 Av. colonel Roche, Postal Code 44346, F-31028; Université de Toulouse, UPS-OMP, Toulouse, France

19. INAF-Osservatorio Astronomico di Trieste, Via G. B Tiepolo 11, I-34143; IFPU-Institute for Fundamental Physics of the Universe, Via Beirut 2, I-34014 Trieste, Italy

20. Department of Physics, University of Arizona, 1118 E. Fourth St, Tucson, AZ 85721, USA

21. Shanghai Astronomical Observatory (SHAO), Nandan Road 80, Shanghai 200030, China

22. Museu de Astronomia e Ciências Afins (MAST), Rua General Bruce 586, 20921-030 Rio de Janeiro, Brasil

23. Department of Physics, PO Box 35 (YFL), FI-40014 University of Jyväskylä, Finland

24. Excellence Cluster Origins, Boltzmannstraße 2, D-85748 Garching, Germany

Abstract

ABSTRACT The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at 0.35 < z < 0.65. It was selected from ROSAT data in the 10 000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX programme on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ lensfit shape measurement and perform a conservative colour–space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large-scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope α, normalization β, and scatter σln λ|μ of our richness–mass scaling relation model in log-space: ${\langle {\rm In}\,\, \lambda\!\!\mid\!\!\mu\rangle = \alpha\mu + \beta,} $ with μ = ln (M200c/Mpiv), and Mpiv = 1014.81M⊙. We find a slope $\alpha = 0.49^{+0.20}_{-0.15}$, normalization $\exp (\beta) = 84.0^{+9.2}_{-14.8}$, and $\sigma _{\ln \lambda | \mu } = 0.17^{+0.13}_{-0.09}$ using CFHT richness estimates. In comparison to other weak lensing richness–mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range (0.0 < z < 0.65) and with different cluster selection (X-ray, Sunyaev–Zeldovich, and optical).

Funder

College of Natural Resources and Sciences, Humboldt State University

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. Impact of property covariance on cluster weak lensing scaling relations;Monthly Notices of the Royal Astronomical Society;2024-04-11

2. Euclid preparation;Astronomy & Astrophysics;2024-01

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4. CODEX: Role of velocity substructure in the scaling relations of galaxy clusters;Astronomy & Astrophysics;2023-08

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