Issue |
A&A
Volume 695, March 2025
|
|
---|---|---|
Article Number | A49 | |
Number of page(s) | 24 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/202451516 | |
Published online | 05 March 2025 |
Galaxy cluster matter profiles
I. Self-similarity, mass calibration, and observable-mass relation validation employing cluster mass posteriors
1
University Observatory, Faculty of Physics, Ludwig-Maximilians-Universitat, Scheinerstr. 1, 81679 Munich, Germany
2
Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, 85748 Garching, Germany
3
Universitat Innsbruck, Institut fur Astro- und Teilchenphysik, Technikerstr. 25/8, 6020 Innsbruck, Austria
4
Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ, 20921-400, Brazil
5
Fermi National Accelerator Laboratory, PO Box 500, Batavia, IL, 60510, USA
6
Department of Physics, University of Michigan, Ann Arbor, MI, 48109, USA
7
Instituto de Física Teórica, Universidade Estadual Paulista, São Paulo, Brazil
8
Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK
9
Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton, BN1 9QH, UK
10
Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
11
Instituto de Astrofisica de Canarias, E-38205 La Laguna, Tenerife, Spain
12
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra, (Barcelona), Spain
13
Astronomy Unit, Department of Physics, University of Trieste, Via Tiepolo 11, I-34131 Trieste, Italy
14
INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34143 Trieste, Italy
15
Institute for Fundamental Physics of the Universe, Via Beirut 2, 34014 Trieste, Italy
16
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
17
Department of Physics, IIT Hyderabad, Kandi, Telangana, 502285, India
18
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA, 91109, USA
19
Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, 60637, USA
20
Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
21
Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain
22
Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
23
Center for Astrophysical Surveys, National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL, 61801, USA
24
Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL, 61801, USA
25
Santa Cruz Institute for Particle Physics, Santa Cruz, CA, 95064, USA
26
Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH, 43210, USA
27
Department of Physics, The Ohio State University, Columbus, OH, 43210, USA
28
Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA, 02138, USA
29
Australian Astronomical Optics, Macquarie University, North Ryde, NSW, 2113, Australia
30
Lowell Observatory, 1400 Mars Hill Rd, Flagstaff, AZ, 86001, USA
31
Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP, 05314-970, Brazil
32
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
33
LPSC Grenoble – 53, Avenue des Martyrs, 38026 Grenoble, France
34
Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain
35
Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ, 08544, USA
36
Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ, 20921-400, Brazil
37
Department of Physics, Northeastern University, Boston, MA, 02115, USA
38
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain
39
School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK
40
Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN, 37831, USA
41
Argonne National Laboratory, 9700 S Cass Ave, Lemont, IL, 60439, USA
42
Department of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA, 94720, USA
43
Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA
⋆ Corresponding author; aditya.singh@physik.lmu.de
Received:
15
July
2024
Accepted:
29
January
2025
We present a study of the weak lensing inferred matter profiles ΔΣ(R) of 698 South Pole Telescope (SPT) thermal Sunyaev-Zel’dovich effect (tSZE) selected and MCMF optically confirmed galaxy clusters in the redshift range 0.25 < z < 0.94 that have associated weak gravitational lensing shear profiles from the Dark Energy Survey (DES). Rescaling these profiles to account for the mass dependent size and the redshift dependent density produces average rescaled matter profiles ΔΣ(R/R200c)/(ρcritR200c) with a lower dispersion than the unscaled ΔΣ(R) versions, indicating a significant degree of self-similarity. Galaxy clusters from hydrodynamical simulations also exhibit matter profiles that suggest a high degree of self-similarity, with RMS variation among the average rescaled matter profiles with redshift and mass falling by a factor of approximately six and 23, respectively, compared to the unscaled average matter profiles. We employed this regularity in a new Bayesian method for weak lensing mass calibration that employs the so-called cluster mass posterior P(M200|ζ̂, λ̂, z), which describes the individual cluster masses given their tSZE (ζ̂) and optical (λ̂, z) observables. This method enables simultaneous constraints on richness λ-mass and tSZE detection significance ζ-mass relations using average rescaled cluster matter profiles. We validated the method using realistic mock datasets and present observable-mass relation constraints for the SPT×DES sample, where we constrained the amplitude, mass trend, redshift trend, and intrinsic scatter. Our observable-mass relation results are in agreement with the mass calibration derived from the recent cosmological analysis of the SPT×DES data based on a cluster-by-cluster lensing calibration. Our new mass calibration technique offers a higher efficiency when compared to the single cluster calibration technique. We present new validation tests of the observable-mass relation that indicate the underlying power-law form and scatter are adequate to describe the real cluster sample but that also suggest a redshift variation in the intrinsic scatter of the λ-mass relation may offer a better description. In addition, the average rescaled matter profiles offer high signal-to-noise ratio (S/N) constraints on the shape of real cluster matter profiles, which are in good agreement with available hydrodynamical ΛCDM simulations. This high S/N profile contains information about baryon feedback, the collisional nature of dark matter, and potential deviations from general relativity.
Key words: gravitational lensing: weak / galaxies: clusters: general / large-scale structure of Universe
© The Authors 2025
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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