CHEX-MATE: The intracluster medium entropy distribution in the gravity-dominated regime
- Creators
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Riva, G.1, 2
- Pratt, G. W.3
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Rossetti, M.1
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Bartalucci, I.1
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Kay, S. T.4
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Rasia, E.5, 6
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Gavazzi, R.7, 8, 9
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Umetsu, K.10
- Arnaud, M.3
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Balboni, M.1, 11
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Bonafede, A.12, 13
- Bourdin, H.14, 15
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De Grandi, S.16
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De Luca, F.14, 15
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Eckert, D.17
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Ettori, S.18
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Gaspari, M.19
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Gastaldello, F.1
- Ghirardini, V.18
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Ghizzardi, S.1
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Gitti, M.12, 13
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Lovisari, L.1, 20
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Maughan, B. J.21
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Mazzotta, P.14, 15
- Molendi, S.1
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Pointecouteau, E.22
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Sayers, Jack23
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Sereno, M.18
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Towler, I.4
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1.
Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano
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2.
University of Milan
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3.
University of Paris
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4.
University of Manchester
- 5. INAF, Osservatorio di Trieste, Via Tiepolo 11, 34131, Trieste, Italy
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6.
Institute for Fundamental Physics of the Universe
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7.
Laboratoire d'Astrophysique de Marseille
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8.
Sorbonne University
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9.
Institut d'Astrophysique de Paris
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10.
Institute of Astronomy and Astrophysics, Academia Sinica
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11.
University of Insubria
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12.
University of Bologna
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13.
Istituto di Radioastronomia di Bologna
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14.
University of Rome Tor Vergata
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15.
INFN Sezione di Roma II
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16.
Brera Astronomical Observatory
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17.
University of Geneva
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18.
National Institute for Astrophysics
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19.
University of Modena and Reggio Emilia
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20.
Harvard-Smithsonian Center for Astrophysics
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21.
University of Bristol
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22.
Research Institute in Astrophysics and Planetology
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23.
California Institute of Technology
Abstract
We characterise the intracluster gas entropy profiles of 32 very high-mass (M500 > 7.75 × 1014 M⊙) Planck SZ-detected galaxy clusters (HIGHMz), selected from the CHEX-MATE sample, allowing us to study the intracluster medium (ICM) entropy distribution in a regime where non-gravitational effects are expected to be minimised. Using XMM-Newton measurements, we determined the entropy profiles up to ∼R500 for all objects. We assessed the relative role of gas density and temperature measurements on the uncertainty in entropy reconstruction, showing that in the outer regions the largest contribution comes from the temperature. The scaled profiles exhibit a large dispersion in the central regions, but converge rapidly to the value expected from simple gravitational collapse beyond the core regions. We quantified the correlation between the ICM morphological parameters and scaled entropy as a function of radius, showing that centrally peaked objects have low central entropy, while morphologically disturbed objects have high central entropy. We compared the scaled HIGHMz entropy profiles to results from other observational samples, finding differences in normalisation, which appear linked to the average mass of the samples in question. Combining HIGHMz with other samples, we found that a weaker mass dependence than self-similar in the scaling (Am ∼ −0.25) allows us to minimise the dispersion in the radial range [0.3 − 0.8] R500 for clusters spanning over a decade in mass. The deviation from self-similar predictions is radially dependent and is more pronounced at small and intermediate radii than at R500. We also investigated the distribution of central entropy K0, finding no evidence for bimodality in the data and outer slope α, which peaks at α ∼ 1.1 with tails at both low and high α that correlate with dynamical state. Using weak-lensing masses for half of the sample, we found an indication for a small suppression of the scatter (∼30%) beyond the core when using masses derived from YX in the rescaling. Finally, we compared our results to recent cosmological numerical simulations from THE THREE HUNDRED and MACSIS, finding good agreement with the observational data in this mass regime. These results provide a robust observational benchmark in the gravity-dominated regime, and will serve as a future reference for samples at lower masses, higher redshifts, and for ongoing work using cosmological numerical simulations.
Copyright and License
© 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.
Acknowledgement
We thank the anonymous referee for useful comments, which have improved our paper. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The research has received funding from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement n. 871158). This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #565 “Multi-Wavelength Studies of the Culmination of Structure Formation in the Universe”. G.R. acknowledges C. Grillo for useful discussions. G.R., M.R., I.B., H.B., S.D.G., F.D.L., S.E., F.G., S.G., L.L., P.M. and S.M. acknowledge the financial contribution from the contracts Prin-MUR 2022, supported by Next Generation EU (n.20227RNLY3 The concordance cosmological model: stress-tests with galaxy clusters), ASI-INAF Athena 2019-27-HH.0, “Attività di Studio per la comunità scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare” (Accordo Attuativo ASI-INAF n. 2017-14-H.0). G.W.P acknowledges long-term support from CNES, the French space agency. K.U. acknowledges support from the National Science and Technology Council of Taiwan (grant NSTC 112-2112-M-001-027-MY3) and the Academia Sinica Investigator Award (grant AS-IA-112-M04). L.L. also acknowledges support from INAF mini grant 1.05.12.04.01. M.S. acknowledges financial contributions from the contracts Prin-MUR 2022 supported by Next Generation EU (M4.C2.1.1, n.20227RNLY3 The concordance cosmological model: stress-tests with galaxy clusters) and INAF Theory Grant 2023: Gravitational lensing detection of matter distribution at galaxy cluster boundaries and beyond (1.05.23.06.17). H.B., P.M., and F.D.L. acknowledge financial contribution from the contracts ASI-INAF Athena 2019-27-HH.0, “Attività di Studio per la comunità scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare” (Accordo Attuativo ASI-INAF n. 2017-14- H.0), support from INFN through the InDark initiative, from “Tor Vergata” Grant “SUPERMASSIVE-Progetti Ricerca Scientifica di Ateneo 2021” and from Fondazione ICSC, Spoke 3 Astrophysics and Cosmos Observations. National Recovery and Resilience Plan (Piano Nazionale di Ripresa e Resilienza, PNRR) Project ID CN00000013 ‘Italian Research Center on High Performance Computing, Big Data and Quantum Computing’ funded by MUR Missione 4 Componente 2 Investimento 1.4: Potenziamento strutture di ricerca e creazione di “campioni nazionali di R&S (M4C2-19 )” - Next Generation EU (NGEU). H.B., P.M. and F.D.L. also acknowledge the financial contribution from the contract PrinMUR 2022 supported by Next Generation EU (n.20227RNLY3 The concordance cosmological model: stress-tests with galaxy clusters). Ma.G. acknowledges support from the ERC Consolidator Grant BlackHoleWeather (101086804). B.J.M acknowledges support from Science and Technology Facilities Council grant ST/Y002008/1. E.P. acknowledges the support of the French Agence Nationale de la Recherche (ANR), under grant ANR-22-CE31-0010 (project BATMAN). J.S. was supported by NASA Astrophysics Data Analysis Program (ADAP) Grant 80NSSC21K1571.
Software References
We made use of the following software packages: FTOOLS (Blackburn 1995), DS9 (Joye & Mandel 2003), and several python libraries, such as numpy (Harris et al. 2020), matplotlib (Hunter 2007), Astropy (Astropy Collaboration 2013, 2018), PyMC (Abril-Pla et al. 2023).
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Additional details
- National Aeronautics and Space Administration
- Astrophysics Data Analysis Program (ADAP) 80NSSC21K1571
- Available
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2024-11-25Published online
- Publication Status
- Published