Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles

I. Bartalucci; S. Molendi; E. Rasia; G. W. Pratt; M. Arnaud; M. Rossetti; F. Gastaldello; D. Eckert; M. Balboni; S. Borgani; H. Bourdin; M. G. Campitiello; S. De Grandi; M. De Petris; R. T. Duffy; S. Ettori; A. Ferragamo; M. Gaspari; R. Gavazzi; S. Ghizzardi; A. Iqbal; S. T. Kay; L. Lovisari; P. Mazzotta; B. J. Maughan; E. Pointecouteau; G. Riva; M. Sereno

doi:10.1051/0004-6361/202346189

Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles

I. Bartalucci^*, S. Molendi, E. Rasia, G. W. Pratt, M. Arnaud, M. Rossetti, F. Gastaldello, D. Eckert, M. Balboni, S. Borgani, H. Bourdin, M. G. Campitiello, S. De Grandi, M. De Petris, R. T. Duffy, S. Ettori, A. Ferragamo, M. Gaspari, R. Gavazzi, S. GhizzardiA. Iqbal, S. T. Kay, L. Lovisari, P. Mazzotta, B. J. Maughan, E. Pointecouteau, G. Riva, M. Sereno

^*Corresponding author for this work

School of Physics

Research output: Contribution to journal › Article (Academic Journal) › peer-review

17 Citations (Scopus)

Abstract

We investigate the statistical properties and the origin of the scatter within the spatially resolved surface brightness profiles of the CHEX-MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects have been drawn from the Planck SZ catalogue and cover a wide range of masses, M$_{500}=[2-15] \times 10^{14} $M$_{\odot}$, and redshift, z=[0.05,0.6]. We derived the surface brightness and emission measure profiles and determined the statistical properties of the full sample. We found that there is a critical scale, R$\sim 0.4 R_{500}$, within which morphologically relaxed and disturbed object profiles diverge. The median of each sub-sample differs by a factor of $\sim 10$ at $0.05\,R_{500}$. There are no significant differences between mass- and redshift-selected sub-samples once proper scaling is applied. We compare CHEX-MATE with a sample of 115 clusters drawn from the The Three Hundred suite of cosmological simulations. We found that simulated emission measure profiles are systematically steeper than those of observations. For the first time, the simulations were used to break down the components causing the scatter between the profiles. We investigated the behaviour of the scatter due to object-by-object variation. We found that the high scatter, approximately 110%, at $R

Original language	English
Article number	A179
Journal	Astronomy and Astrophysics
Volume	674
DOIs	https://doi.org/10.1051/0004-6361/202346189
Publication status	Published - 23 Jun 2023

Bibliographical note

Funding Information:
The authors thank the referee for his/her comments. We 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 No. 2017-14-H.0), and from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency.

Funding Information:
The authors thank the referee for his/her comments. We 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 No. 2017-14-H.0), and from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency.

Publisher Copyright:
© The Authors 2023.

Keywords

astro-ph.CO

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Bartalucci, I., Molendi, S., Rasia, E., Pratt, G. W., Arnaud, M., Rossetti, M., Gastaldello, F., Eckert, D., Balboni, M., Borgani, S., Bourdin, H., Campitiello, M. G., Grandi, S. D., Petris, M. D., Duffy, R. T., Ettori, S., Ferragamo, A., Gaspari, M., Gavazzi, R., ... Sereno, M. (2023). Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles. Astronomy and Astrophysics, 674, Article A179. https://doi.org/10.1051/0004-6361/202346189

@article{6e8f981db18a42a9a74c2d2977a284f8,

title = "Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles",

abstract = "We investigate the statistical properties and the origin of the scatter within the spatially resolved surface brightness profiles of the CHEX-MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects have been drawn from the Planck SZ catalogue and cover a wide range of masses, M\$\_\{500\}=[2-15] \textbackslash{}times 10\textasciicircum{}\{14\} \$M\$\_\{\textbackslash{}odot\}\$, and redshift, z=[0.05,0.6]. We derived the surface brightness and emission measure profiles and determined the statistical properties of the full sample. We found that there is a critical scale, R\$\textbackslash{}sim 0.4 R\_\{500\}\$, within which morphologically relaxed and disturbed object profiles diverge. The median of each sub-sample differs by a factor of \$\textbackslash{}sim 10\$ at \$0.05\textbackslash{},R\_\{500\}\$. There are no significant differences between mass- and redshift-selected sub-samples once proper scaling is applied. We compare CHEX-MATE with a sample of 115 clusters drawn from the The Three Hundred suite of cosmological simulations. We found that simulated emission measure profiles are systematically steeper than those of observations. For the first time, the simulations were used to break down the components causing the scatter between the profiles. We investigated the behaviour of the scatter due to object-by-object variation. We found that the high scatter, approximately 110\%, at \$R",

keywords = "astro-ph.CO",

author = "I. Bartalucci and S. Molendi and E. Rasia and Pratt, \{G. W.\} and M. Arnaud and M. Rossetti and F. Gastaldello and D. Eckert and M. Balboni and S. Borgani and H. Bourdin and Campitiello, \{M. G.\} and Grandi, \{S. De\} and Petris, \{M. De\} and Duffy, \{R. T.\} and S. Ettori and A. Ferragamo and M. Gaspari and R. Gavazzi and S. Ghizzardi and A. Iqbal and Kay, \{S. T.\} and L. Lovisari and P. Mazzotta and Maughan, \{B. J.\} and E. Pointecouteau and G. Riva and M. Sereno",

note = "Funding Information: The authors thank the referee for his/her comments. We acknowledge financial contribution from the contracts ASI-INAF Athena 2019-27-HH.0, “Attivit{\`a} di Studio per la comunit{\`a} scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare” (Accordo Attuativo ASI-INAF No. 2017-14-H.0), and from the European Union{\textquoteright}s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency. Funding Information: The authors thank the referee for his/her comments. We acknowledge financial contribution from the contracts ASI-INAF Athena 2019-27-HH.0, “Attivit{\`a} di Studio per la comunit{\`a} scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare” (Accordo Attuativo ASI-INAF No. 2017-14-H.0), and from the European Union{\textquoteright}s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency. Publisher Copyright: {\textcopyright} The Authors 2023.",

year = "2023",

month = jun,

day = "23",

doi = "10.1051/0004-6361/202346189",

language = "English",

volume = "674",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Bartalucci, I, Molendi, S, Rasia, E, Pratt, GW, Arnaud, M, Rossetti, M, Gastaldello, F, Eckert, D, Balboni, M, Borgani, S, Bourdin, H, Campitiello, MG, Grandi, SD, Petris, MD, Duffy, RT, Ettori, S, Ferragamo, A, Gaspari, M, Gavazzi, R, Ghizzardi, S, Iqbal, A, Kay, ST, Lovisari, L, Mazzotta, P, Maughan, BJ, Pointecouteau, E, Riva, G & Sereno, M 2023, 'Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles', Astronomy and Astrophysics, vol. 674, A179. https://doi.org/10.1051/0004-6361/202346189

TY - JOUR

T1 - Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles

AU - Bartalucci, I.

AU - Molendi, S.

AU - Rasia, E.

AU - Pratt, G. W.

AU - Arnaud, M.

AU - Rossetti, M.

AU - Gastaldello, F.

AU - Eckert, D.

AU - Balboni, M.

AU - Borgani, S.

AU - Bourdin, H.

AU - Campitiello, M. G.

AU - Grandi, S. De

AU - Petris, M. De

AU - Duffy, R. T.

AU - Ettori, S.

AU - Ferragamo, A.

AU - Gaspari, M.

AU - Gavazzi, R.

AU - Ghizzardi, S.

AU - Iqbal, A.

AU - Kay, S. T.

AU - Lovisari, L.

AU - Mazzotta, P.

AU - Maughan, B. J.

AU - Pointecouteau, E.

AU - Riva, G.

AU - Sereno, M.

N1 - Funding Information: The authors thank the referee for his/her comments. We 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 No. 2017-14-H.0), and from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency. Funding Information: The authors thank the referee for his/her comments. We 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 No. 2017-14-H.0), and from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement No. 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). The results reported in this article are based on data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GWP acknowledges financial support from CNES, the French space agency. Publisher Copyright: © The Authors 2023.

PY - 2023/6/23

Y1 - 2023/6/23

N2 - We investigate the statistical properties and the origin of the scatter within the spatially resolved surface brightness profiles of the CHEX-MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects have been drawn from the Planck SZ catalogue and cover a wide range of masses, M$_{500}=[2-15] \times 10^{14} $M$_{\odot}$, and redshift, z=[0.05,0.6]. We derived the surface brightness and emission measure profiles and determined the statistical properties of the full sample. We found that there is a critical scale, R$\sim 0.4 R_{500}$, within which morphologically relaxed and disturbed object profiles diverge. The median of each sub-sample differs by a factor of $\sim 10$ at $0.05\,R_{500}$. There are no significant differences between mass- and redshift-selected sub-samples once proper scaling is applied. We compare CHEX-MATE with a sample of 115 clusters drawn from the The Three Hundred suite of cosmological simulations. We found that simulated emission measure profiles are systematically steeper than those of observations. For the first time, the simulations were used to break down the components causing the scatter between the profiles. We investigated the behaviour of the scatter due to object-by-object variation. We found that the high scatter, approximately 110%, at $R

AB - We investigate the statistical properties and the origin of the scatter within the spatially resolved surface brightness profiles of the CHEX-MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects have been drawn from the Planck SZ catalogue and cover a wide range of masses, M$_{500}=[2-15] \times 10^{14} $M$_{\odot}$, and redshift, z=[0.05,0.6]. We derived the surface brightness and emission measure profiles and determined the statistical properties of the full sample. We found that there is a critical scale, R$\sim 0.4 R_{500}$, within which morphologically relaxed and disturbed object profiles diverge. The median of each sub-sample differs by a factor of $\sim 10$ at $0.05\,R_{500}$. There are no significant differences between mass- and redshift-selected sub-samples once proper scaling is applied. We compare CHEX-MATE with a sample of 115 clusters drawn from the The Three Hundred suite of cosmological simulations. We found that simulated emission measure profiles are systematically steeper than those of observations. For the first time, the simulations were used to break down the components causing the scatter between the profiles. We investigated the behaviour of the scatter due to object-by-object variation. We found that the high scatter, approximately 110%, at $R

KW - astro-ph.CO

U2 - 10.1051/0004-6361/202346189

DO - 10.1051/0004-6361/202346189

M3 - Article (Academic Journal)

SN - 0004-6361

VL - 674

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A179

ER -

Chex-mate: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles

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