Suzaku X-Ray Observations of the Accreting NGC 4839 Group of Galaxies and a Radio Relic in the Coma Cluster

被引：38

作者：

Akamatsu, Hiroki ^{[1
]}

Inoue, Susumu ^{[2
,3
]}

Sato, Takuya ^{[4
]}

Matsusita, Kyoko ^{[4
]}

Ishisaki, Yoshitaka ^{[5
]}

Sarazin, Craig L. ^{[6
]}

机构：

[1] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands

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

[3] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[4] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan

[5] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan

[6] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN | 2013年 / 65卷 / 04期

关键词：

galaxies:; clusters:; individual; (Coma; NGC; 4839); galaxies: intergalactic medium; shock waves; X-rays: galaxies: clusters; LARGE-SCALE STRUCTURE; XMM-NEWTON OBSERVATIONS; HIGH-ENERGY PROTONS; PARTICLE-ACCELERATION; TEMPERATURE PROFILES; INTRACLUSTER MEDIUM; SHOCK-WAVES; NEARBY CLUSTERS; EXTENDED SOURCE; STAR-FORMATION;

D O I：

10.1093/pasj/65.4.89

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Based on Suzaku X-ray observations, we studied the hot gas around the NGC 4839 group of galaxies and a radio relic in the outskirts of the Coma cluster. We found a gradual decline in the gas temperature from 5 keV around NGC 4839 to 3.6 keV at the radio relic, across which there is a further, steeper drop down to 1.5 keV. This drop as well as the observed surface brightness profile are consistent with a shock with Mach number M = 2.2 +/- 0.5 and velocity upsilon(s) = (1410 +/- 110) km s(-1). A lower limit of B > 0.33 mu G was derived based on the magnetic field strength around the relic from the upper limits to inverse Compton X-ray emission. Although this suggests that the non-thermal electrons responsible for the relic are generated by diffusive shock acceleration (DSA), the relation between the measured Mach number and the electron spectrum inferred from radio observations are inconsistent with that expected from the simplest, test-particle theory of DSA. Nevertheless, DSA is still viable if it is initiated by the injection of a pre-existing population of non-thermal electrons. Combined with previous measurements, the temperature profile of Coma in the southwest direction is shallower outside NGC 4839, and also slightly shallower in the outermost region. The metal abundance around NGC 4839 is confirmed to be higher than that in its vicinity, implying a significant peak in the abundance profile that decreases to 0.2 solar toward the outskirts. We interpret these facts as being due to ram pressure stripping of metal-enriched gas from NGC 4839 as it falls into Coma. The relic shock may result from the combined interaction of pre-existing intracluster gas, gas associated with NGC 4839, and cooler gas flowing in from the large-scale structure filament in the southwest.

引用

页数：14

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