Issue |
A&A
Volume 687, July 2024
|
|
---|---|---|
Article Number | A178 | |
Number of page(s) | 27 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/202348615 | |
Published online | 09 July 2024 |
The SRG/eROSITA All-Sky Survey
Dark Energy Survey year 3 weak gravitational lensing by eRASS1 selected galaxy clusters
1
Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstr. 25/8, 6020 Innsbruck, Austria
e-mail: sebastian.grandis@uibk.ac.at
2
Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748 Garching, Germany
3
Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany
4
Argelander-Institut für Astronomie (AIfA), Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
5
Linköpings Universitet, Institutionen för Systemteknik, Linköpings Universitet, Linköping, 581 83
Sweden
6
Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA
UK
7
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA
UK
8
Physics Department, University of Wisconsin-Madison, Madison, WI, 53706
USA
9
Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL, 60439
USA
10
Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA, 19104
USA
11
Department of Physics, Carnegie Mellon University, Pittsburgh, PA, 15312
USA
12
Instituto de Astrofisica de Canarias, 38205 La Laguna, Tenerife, Spain
13
Laboratório Interinstitucional de e-Astronomia – LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ, 20921-400
Brazil
14
Universidad de La Laguna, Dpto. Astrofísica, 38206 La Laguna, Tenerife, Spain
15
Center for Astrophysical Surveys, National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL, 61801
USA
16
Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL, 61801
USA
17
Physics Department, William Jewell College, Liberty, MO, 64068
USA
18
Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, 60637
USA
19
Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, 60637
USA
20
Department of Physics, Duke University Durham, Durham, NC, 27708
USA
21
Department of Physics, National Cheng Kung University, 70101 Tainan, Taiwan
22
NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD, 20771
USA
23
IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
24
Jodrell Bank Center for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL
UK
25
School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072
Australia
26
Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720
USA
27
Fermi National Accelerator Laboratory, PO Box 500 Batavia, IL, 60510
USA
28
NSF AI Planning Institute for Physics of the Future, Carnegie Mellon University, Pittsburgh, PA, 15213
USA
29
Université Grenoble Alpes, CNRS, LPSC-IN2P3, 38000 Grenoble, France
30
Department of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON, N2L 3G1
Canada
31
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA, 91109
USA
32
SLAC National Accelerator Laboratory, Menlo Park, CA, 94025
USA
33
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain
34
Department of Physics and Astronomy, University of Sussex, Pevensey Building, Brighton, BN1 9QH
UK
35
School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA
UK
36
Department of Astronomy, University of Geneva, ch. d’Écogia 16, 1290 Versoix, Switzerland
37
Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, PO Box 2450 Stanford, CA, 94305
USA
38
Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge, CB3 0WA
UK
39
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA, 94305
USA
40
Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859 Campinas, SP, Brazil
41
Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima, 739-8526
Japan
42
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima, 739-8526
Japan
43
Core Research for Energetic Universe, Hiroshima University, 1-3-1, Kagamiyama, Higashi-Hiroshima, Hiroshima, 739-8526
Japan
44
Department of Physics, University of Genova and INFN, Via Dodecaneso 33, 16146 Genova, Italy
45
Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH, 43210
USA
46
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain
47
Brookhaven National Laboratory, Bldg 510, Upton, NY, 11973
USA
48
Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY, 11794
USA
49
Département de Physique Théorique and Center for Astroparticle Physics (CAP), University of Geneva, 24 quai Ernest Ansermet, 1211 Genève, Switzerland
50
Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, 31400 Toulouse, France
51
Department of Physics, Boise State University, Boise, ID, 83725
USA
52
McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, 15213
USA
53
Department of Physics, University of Michigan, Ann Arbor, MI, 48109
USA
54
Astronomy Unit, Department of Physics, University of Trieste, Via Tiepolo 11, 34131 Trieste, Italy
55
INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy
56
Institute for Fundamental Physics of the Universe, Via Beirut 2, 34014 Trieste, Italy
57
Santa Cruz Institute for Particle Physics, Santa Cruz, CA, 95064
USA
58
Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN, 37831
USA
59
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
60
Department of Physics, IIT Hyderabad, Kandi, Telangana, 502285
India
61
Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT
UK
62
Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern 0315 Oslo, Norway
63
Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
64
Department of Physics, The Ohio State University, Columbus, OH, 43210
USA
65
Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA, 02138
USA
66
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
67
Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ, 20921-400
Brazil
68
School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ
UK
Received:
15
November
2023
Accepted:
27
March
2024
Context. Number counts of galaxy clusters across redshift are a powerful cosmological probe if a precise and accurate reconstruction of the underlying mass distribution is performed – a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing (WL) by clusters has become the method of choice for this measurement.
Aims. We measured and validated the WL signature in the shape of galaxies observed in the first three years of the Dark Energy Survey (DES Y3) caused by galaxy clusters and groups selected in the first all-sky survey performed by SRG (Spectrum Roentgen Gamma)/eROSITA (eRASS1). These data were then used to determine the scaling between the X-ray photon count rate of the clusters and their halo mass and redshift.
Methods. We empirically determined the degree of cluster member contamination in our background source sample. The individual cluster shear profiles were then analyzed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we performed mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allowed us to establish that hydrodynamical modeling uncertainties at low lens redshifts (z < 0.6) are the dominant systematic limitation. At high lens redshift, the uncertainties of the sources’ photometric redshift calibration dominate.
Results. With regard to the X-ray count rate to halo mass relation, we determined its amplitude, its mass trend, the redshift evolution of the mass trend, the deviation from self-similar redshift evolution, and the intrinsic scatter around this relation.
Conclusions. The mass calibration analysis performed here sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments, opening the way for the cluster cosmological exploitation of future optical and NIR surveys like Euclid and LSST.
Key words: gravitational lensing: weak / large-scale structure of Universe / X-rays: galaxies: clusters
© The Authors 2024
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.
This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.