The XMM Cluster Outskirts Project (X-COP): Thermodynamic properties of the intracluster medium out to R200 in Abell 2319

被引：72

作者：

Ghirardini, V. ^{[1
,2
]}

Ettori, S. ^{[2
,3
]}

Eckert, D. ^{[4
,5
]}

Molendi, S. ^{[6
]}

Gastaldello, F. ^{[6
]}

Pointecouteau, E. ^{[7
,8
]}

Hurier, G. ^{[9
,10
]}

Bourdin, H. ^{[11
,12
]}

机构：

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

[2] Osservatorio Astron Bologna, INAF, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

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

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

[5] Univ Geneva, Dept Astron, Ch Ec 16, CH-1290 Versoix, Switzerland

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

[7] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[8] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France

[9] Ctr Estudios Fis Cosmos Aragon, Plaza San Juan 1,Planta 2, Teruel 44001, Spain

[10] Univ Paris Sud 11, CNRS, UMR8617, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France

[11] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

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

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 614卷

关键词：

galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters; intergalactic medium; GALAXY CLUSTERS; SUNYAEV-ZELDOVICH; HYDRODYNAMICAL SIMULATIONS; RAY; GAS; PROFILES; MASS; TEMPERATURE; ENTROPY; CHANDRA;

D O I：

10.1051/0004-6361/201731748

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We present the joint analysis of the X-ray and Sunyaev-Zel'dovich (SZ) signals in Abell 2319, the galaxy cluster with the highest signal-to-noise ratio in SZ Planck maps and that has been surveyed within our XMM-Newton Cluster Outskirts Project (X-COP), a very large program which aims to grasp the physical condition in 12 local (z<0.1)and massive (M-200 > 3x10(14) M-circle dot) galaxy clusters out to R-200 and beyond. Methods. We recover the profiles of the thermodynamic properties by the geometrical deprojection of the X-ray surface brightness, of the SZ Comptonization parameter, and accurate and robust spectroscopic measurements of the gas temperature out to 3.2 Mpc (1.6 R-200), 4 Mpc (2 R-200), and 1.6 Mpc (0.8 R-200), respectively. We resolve the clumpiness of the gas density to be below 20% over the entire observed volume. We also demonstrate that most of this clumpiness originates from the ongoing merger and can be associated with large-scale inhomogeneities (the "residual" clumpiness). We estimate the total mass through the hydrostatic equilibrium equation. This analysis is done both in azimuthally averaged radial bins and in eight independent angular sectors, enabling us to study in detail the azimuthal variance of the recovered properties. Results. Given the exquisite quality of the X-ray and SZ datasets, their radial extension, and their complementarity, we constrain at R-200 the total hydrostatic mass, modelled with a Navarro-Frenk-White profile at very high precision (M-200 = 10 : 7 +/- 0 : 5(stat.) +/- 0 : 9(syst.) x 10(14) M-circle dot). We identify the ongoing merger and how it is affecting differently the gas properties in the resolved azimuthal sectors. We have several indications that the merger has injected a high level of non- thermal pressure in this system: the clumping free density profile is above the average profile obtained by stacking Rosat/PSPC observations; the gas mass fraction recovered using our hydrostatic mass profile exceeds the expected cosmic gas fraction beyond R-500; the pressure profile is flatter than the fit obtained by the Planck Collaboration; the entropy profile is flatter than the mean profile predicted from non-radiative simulations; the analysis in azimuthal sectors has revealed that these deviations occur in a preferred region of the cluster. All these tensions are resolved by requiring a relative support of about 40% from non-thermal to the total pressure at R-200.

引用

页数：22

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