Galaxy cluster matter profiles

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 / R 200c )/( ρ crit R 200c ) 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 ( M 200 |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.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-03-01
DOI
https://doi.org/10.1051/0004-6361/202451516
Citations
3
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
3.46

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article

Galaxy cluster matter profiles

A. Pieres, D. Sanchez Cid, J. García-Bellido, S. Bocquet et al.
3 citations
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
3.46
article

Galaxy cluster matter profiles

A. Pieres, D. Sanchez Cid, J. García-Bellido, S. Bocquet, S. Allam, L. N. da Costa, Amitesh Singh, R. Miquel, S. Grandis, Kathy Romer, J. L. Marshall, J. Myles, O. Alves, P. Wiseman, K. Honscheid, G. Gutierrez, J. Carretero, D. J. James, Eusebio Sanchez, E. Suchyta, J. Mena-Fernández, V. Vikram, A. Carnero Rosell, S. Samuroff, ENRIQUE GAZTAÑAGA, R. A. Gruendl, J. García-Bellido, F. Menanteau, J. J. Mohr, M. Aguena, M. E. C. Swanson, M. Lima, M. E. S. Pereira, H. T. Diehl, F. Andrade-Oliveira, M. Costanzi, D. L. Tucker, Matthias Klein, C. T. Davies, M. Smith, K. Kuehn, P. Doel, J. Frieman, S. Desai, G. Tarle, I Sevilla-Noarbe, N. Weaverdyck, S Everett, B. Flaugher, D. Bacon, S. Bhargava, C. To, Donal Brooks
article en
3 citations

Abstract

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 / R 200c )/( ρ crit R 200c ) 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 ( M 200 |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.

Astronomy and AstrophysicsVol. 695
Institució Catalana de Recerca i Estudis Avançats (ES), Argonne National Laboratory (US), Oak Ridge National Laboratory (US), Northeastern University (US), Fermi National Accelerator Laboratory (US), Institute of Space Sciences (ES), Jet Propulsion Laboratory (US), University of Trieste (IT), Lawrence Berkeley National Laboratory (US), University of Illinois Urbana-Champaign (US), Universität Hamburg (DE), University of Sussex (GB), Universidade de São Paulo (BR), Institute for High Energy Physics (ES), Universität Innsbruck (AT), Princeton University (US), University of Michigan (US), Lowell Observatory (US), Trieste Astronomical Observatory (IT), Mitchell Institute (US), Australian Astronomical Observatory (AU), University of Chicago (US), Valongo Observatory (BR), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), National Center for Supercomputing Applications (US), Laboratoire de Physique Subatomique et de Cosmologie (FR), Laboratório Interinstitucional de e-Astronomia (BR), Institute for Fundamental Physics of the Universe (IT), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), University College London (GB), The Ohio State University (US), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Indian Institute of Technology Hyderabad (IN), Ludwig-Maximilians-Universität München (DE), Universidade Estadual Paulista (Unesp) (BR), Texas A&M University (US), University of California, Berkeley (US), Macquarie University (AU)
National Science Foundation, U.S. Department of Energy, University of Pennsylvania, Ohio State University, University of Chicago, University of Portsmouth, Centres de Recerca de Catalunya, University College London, European Commission, University of Sussex, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Ministério da Ciência, Tecnologia e Inovação, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Max-Planck-Gesellschaft, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos, Ministerio de Ciencia e Innovación, Institut de Física d'Altes Energies, University of Illinois at Urbana-Champaign, Office of Science, Science and Technology Facilities Council, European Regional Development Fund, High Energy Physics, Integrated Electronics Engineering Center, Binghamton University, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, SLAC National Accelerator Laboratory
Openalex Percentile: Top 9%
Galaxies: Formation, Evolution, Phenomena
3.46
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