Non-thermal pressure support in X-COP galaxy clusters

被引：141

作者：

Eckert, D. ^{[1
]}

Ghirardini, V. ^{[2
]}

Ettori, S. ^{[3
,4
]}

Rasia, E. ^{[5
]}

Ffi, V. Bi ^{[5
,6
]}

Pointecouteau, E. ^{[7
]}

Rossetti, M. ^{[8
]}

Molendi, S. ^{[8
]}

Vazza, F. ^{[2
,9
]}

Gastaldello, F. ^{[8
]}

Gaspari, M. ^{[10
]}

De Grandi, S. ^{[11
]}

Ghizzardi, S. ^{[8
]}

Bourdin, H. ^{[12
]}

Tchernin, C. ^{[13
]}

Roncarelli, M. ^{[2
]}

机构：

[1] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[2] Univ Bologna, Dipartimento Fis & Astron, Via Piero Gobetti 93-2, I-40129 Bologna, Italy

[3] INAF, Osservatorio Astrofis & Sci Spazio, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

[4] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[5] INAF, Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste, Italy

[6] Univ Trieste, Dipartimento Fis, Sez Astr, Via Tiepolo 11, I-34131 Trieste, Italy

[7] Univ Toulouse, IRAP, CNRS, CNES,UPS, Toulouse, France

[8] INAF, IASF Milano, Via E Bassini 15, I-20133 Milan, Italy

[9] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-40131 Hamburg, Germany

[10] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

[11] INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy

[12] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy

[13] Heidelberg Univ, Inst Theoret Astrophys, Ctr Astron, Philosophenweg 12, D-69120 Heidelberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 621卷

关键词：

X-rays: galaxies: clusters; large-scale structure of Universe; galaxies: clusters: intracluster medium; galaxies: clusters: general; COSMOLOGICAL PARAMETER CONSTRAINTS; INTRACLUSTER MEDIUM; DARK-MATTER; BARYON CONTENT; STELLAR MASS; TURBULENT MOTIONS; ANALYTICAL-MODEL; GAS; SIMULATIONS; FRACTIONS;

D O I：

10.1051/0004-6361/201833324

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Galaxy clusters are the endpoints of structure formation and are continuously growing through the merging and accretion of smaller structures. Numerical simulations predict that a fraction of their energy content is not yet thermalized, mainly in the form of kinetic motions (turbulence, bulk motions). Measuring the level of non-thermal pressure support is necessary to understand the processes leading to the virialization of the gas within the potential well of the main halo and to calibrate the biases in hydrostatic mass estimates. We present high-quality measurements of hydrostatic masses and intracluster gas fraction out to the virial radius for a sample of 13 nearby clusters with available XMM-Newton and Planck data. We compare our hydrostatic gas fractions with the expected universal gas fraction to constrain the level of non-thermal pressure support. We find that hydrostatic masses require little correction and infer a median non-thermal pressure fraction of similar to 6% and similar to 10% at R-500 and R-200, respectively. Our values are lower than the expectations of hydrodynamical simulations, possibly implying a faster thermalization of the gas. If instead we use the mass calibration adopted by the Planck team, we find that the gas fraction of massive local systems implies a mass bias 1 - b = 0.85 +/- 0.05 for Sunyaev-Zeldovich-derived masses, with some evidence for a mass-dependent bias. Conversely, the high bias required to match Planck cosmic microwave background and cluster count cosmology is excluded by the data at high significance, unless the most massive halos are missing a substantial fraction of their baryons.

引用

页数：11

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