THE TEMPERATURE OF HOT GAS IN GALAXIES AND CLUSTERS: BARYONS DANCING TO THE TUNE OF DARK MATTER

被引：9

作者：

Hansen, Steen H. ^{[1
]}

Maccio, Andrea V. ^{[2
]}

Romano-Diaz, Emilio ^{[3
]}

Hoffman, Yehuda ^{[4
]}

Brueggen, Marcus ^{[5
]}

Scannapieco, Evan ^{[6
]}

Stinson, Greg S. ^{[7
]}

机构：

[1] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark

[2] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[3] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA

[4] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel

[5] Jacobs Univ Bremen, D-28725 Bremen, Germany

[6] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[7] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 734卷 / 01期

基金：

新加坡国家研究基金会;

关键词：

galaxies: clusters: intracluster medium; galaxies: evolution; galaxies: fundamental parameters; methods: numerical; VELOCITY ANISOTROPY; FRAGMENTATION; ENTROPY; ORIGIN; CLOUDS; HALOS; DISC;

D O I：

10.1088/0004-637X/734/1/62

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The temperature profile of hot gas in galaxies and galaxy clusters is largely determined by the depth of the total gravitational potential and thereby by the dark matter (DM) distribution. We use high-resolution hydrodynamical simulations of galaxy formation to derive a surprisingly simple relation between the gas temperature and DM properties. We show that this relation holds not just for galaxy clusters but also for equilibrated and relaxed galaxies at radii beyond the central stellar-dominated region of typically a few kpc. It is then clarified how a measurement of the temperature and density of the hot gas component can lead to an indirect measurement of the DM velocity anisotropy in galaxies. We also study the temperature relation for galaxy clusters in the presence of self-regulated, recurrent active galactic nuclei (AGNs), and demonstrate that this temperature relation even holds outside the inner region of approximate to 30 kpc in clusters with an active AGN.

引用

页数：7

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