Suzaku Observations of AWM 7 Cluster of Galaxies: Temperatures, Abundances, and Bulk Motions
Suzaku Observations of AWM 7 Cluster of Galaxies: Temperatures, Abundances, and Bulk Motions
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DOI：
10.1093/pasj/60.sp1.s333
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发表时间：
2007-07
影响因子：
2.3
通讯作者：
Kosuke Sato;K. Matsushita;Y. Ishisaki;N. Yamasaki;M. Ishida;S. Sasaki;T. Ohashi
中科院分区：
文献类型：
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作者：
Kosuke Sato;K. Matsushita;Y. Ishisaki;N. Yamasaki;M. Ishida;S. Sasaki;T. Ohashi
我们对星系团AWM 7进行了3次观测，分别是中心区域和200东偏和200西偏的区域。温度和丰度分布测量到270 ' 570 h 170 kpc，其对应于0.35r180。团簇内介质（ICM）的温度从中心的3.8 keV略微下降到0.35 r180区域的3.4 keV，表明比附近其他团簇中的温度分布更平坦。在我们的观测中，Si与Fe的丰度比几乎是恒定的，而Mg与Fe的比值随着半径的增加而增加。西部地区的O/Fe比值随半径的增大而增大，东部地区的O/Fe比值随半径的增大而减小，但误差较大。这些特征表明，II型超新星的产物（O和Mg）和Ia型超新星的产物（Si和Fe）之间的富集过程是显着不同的。我们还研究了类He Fe-K线的中心能量的位置移动，以寻找ICM的可能旋转。视线速度差的90%上限被推导为100 V。2000 km/s，这表明AWM 7的椭圆率是由最近的定向气体沿沿着大规模的灯丝下降。
We carried out 3 observations of the cluster of galaxies AWM 7, for the central region and 200-east and 200-west offset regions, with Suzaku. Temperature and abundance profiles were measured out to 270 ' 570 h 1 70 kpc, which corresponded to 0.35r180. The temperature of the intra-cluster medium (ICM) slightly decreased from 3.8 keV at the center to 3.4 keV in the 0.35 r180 region, indicating a flatter profile than those in other nearby clusters. The abundance ratio of Si to Fe was almost constant in our observations, while the Mg-to-Fe ratio increased with radius from the cluster center. The O to Fe ratio in the west region showed an increase with radius, while that in the east region was almost flat, though the errors were relatively large. These features suggest that the enrichment process is significantly different between products of type II supernovae (O and Mg) and those by type Ia supernovae (Si and Fe). We also examined the positional shift of the central energy of a He-like Fe-K line, in search of possible rotation of the ICM. The 90% upper limit for the line-of-sight velocity difference was derived to be ∆v . 2000 km s , suggesting that the ellipticity of AWM 7 is rather caused by a recent directional infall of gas along the large-scale filament.