Issue |
A&A
Volume 700, August 2025
|
|
---|---|---|
Article Number | A15 | |
Number of page(s) | 19 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/202554177 | |
Published online | 25 July 2025 |
Selection function of clusters in Dark Energy Survey year 3 data from cross-matching with South Pole Telescope detections
1
Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstrasse 25, 6020 Innsbruck, Austria
2
Dipartimento di Fisica – Sezione di Astronomia, Università di Trieste, Via Tiepolo 11, 34131 Trieste, Italy
3
INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy
4
IFPU – Institute for Fundamental Physics of the Universe, Via Beirut 2, 34014 Trieste, Italy
5
University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany
6
Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748 Garching, Germany
7
High-Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue., Lemont, IL 60439, USA
8
Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
9
Department of Physics, Southern Methodist University, Dallas, TX 75205, USA
10
Laboratório Interinstitucional de e-Astronomia – LIneA, Av. Pastor Martin Luther King Jr, 126 Del Castilho, Nova América Offices, Torre 3000/sala 817 CEP: 20765-000, Sao Paolo, Brazil
11
Fermi National Accelerator Laboratory, P. O. Box 500 Batavia, IL 60510, USA
12
Physik-Institut, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
13
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
14
Instituto de Astrofisica de Canarias, E-38205 La Laguna, Tenerife, Spain
15
Universidad de La Laguna, Dpto. Astrofisica, E-38206 La Laguna, Tenerife, Spain
16
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain
17
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
18
School of Mathematics and Physics, University of Queensland, Brisbane QLD 4072, Australia
19
Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India
20
California Institute of Technology, 1200 East California Blvd, MC 249-17, Pasadena, CA 91125, USA
21
Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA
22
Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
23
Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain
24
Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK
25
Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
26
Center for Astrophysical Surveys, National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
27
Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA
28
Département de Physique, Université de Montréal, Succ. Centre-Ville, Montréal, Québec H3C 3J7, Canada
29
Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA
30
Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA
31
Department of Physics, The Ohio State University, Columbus, OH 43210, USA
32
Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
33
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
34
LPSC Grenoble –, 53, Avenue des Martyrs, 38026 Grenoble, France
35
Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain
36
Department of Physics, Carnegie Mellon University, Pittsburgh, Pennsylvania 15312, USA
37
Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450 Stanford University, Stanford, CA 94305, USA
38
SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
39
School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia
40
Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton BN1 9QH, UK
41
Department of Physics, Northeastern University, Boston, MA 02115, USA
42
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain
43
Instituto de Física, UFRGS, Caixa Postal 15051, Porto Alegre RS – 91501-970, Brazil
44
Physics Department, Lancaster University, Lancaster LA1 4YB, UK
45
Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany
46
Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA
47
Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
48
Department of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA 94720, USA
49
Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA
50
School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK
⋆ Corresponding author: sebastian.grandis@uibk.ac.at
Received:
18
February
2025
Accepted:
3
June
2025
Context. Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. However, modeling the selection function of such samples is complicated by noncluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination).
Aims. We empirically constrained the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy Survey data with the redMaPPer algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d).
Methods. For matched clusters, we augmented the redMaPPer catalog with the SPT detection significance. For unmatched objects we used the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multiwavelength data, we explored various physically motivated models to describe the relationship between observed richness and halo mass.
Results. Our analysis reveals a clear preference for models with an additional skewed scatter component associated with projection effects over a purely log-normal scatter model. We rule out significant contamination by unvirialized objects at the high-richness end of the sample. While dedicated simulations offer a well-fitting calibration of projection effects, our findings suggest the presence of redshift-dependent trends that these simulations may not have captured. Our findings highlight that modeling the selection function of optically detected clusters remains a complicated challenge that requires a combination of simulation and data-driven approaches.
Key words: methods: statistical / 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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