TWO-PHASE ICM IN THE CENTRAL REGION OF THE RICH CLUSTER OF GALAXIES A1795: A JOINT CHANDRA, XMM-NEWTON, AND SUZAKU VIEW
TWO-PHASE ICM IN THE CENTRAL REGION OF THE RICH CLUSTER OF GALAXIES A1795: A JOINT CHANDRA, XMM-NEWTON, AND SUZAKU VIEW
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丰富星系团 A1795 中心区的两相 ICM：钱德拉、XMM-牛顿和朱雀的联合视图
DOI：
10.1088/0004-637x/749/2/186
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发表时间：
2012-02
期刊：
影响因子：
--
通讯作者：
Zhang, Zhongli
中科院分区：
文献类型：
--
作者：
Gu, Liyi;Makishima, Kazuo;Xu, Haiguang;Gu, Junhua;Kawaharada, Madoka;Nakazawa, Kazuhiro;Qin, Zhenzhen;Wang, Jingying;Wang, Yu;Zhang, Zhongli
基于对钱德拉、xmm -牛顿和Suzaku高质量x射线明亮星系团A1795的数据的详细分析，我们报告了两相星系团内介质（ICM）结构的明确证据，该结构由冷（温度Tc≈2.0-2.2 keV）和热（Th≈5.0-5.7 keV）组成，它们共存并主导了至少在80 kpc中心的x射线发射。第三种弱发射成分（T3≈0.8 keV）也在最内层的144 kpc内被探测到，并被认为是cD星系的一部分星际介质。去投影光谱分析表明，热相和冷相组分的径向温度分布都是平坦的。这些结果与Xu等人报道的ASCA测量结果一致，类似于之前对半人马座星团的发现。通过分析钱德拉数据生成的发射测量比和气体金属丰度图，我们发现在50-100 kpc区域，冷相组分比热相组分更富金属，这与M87的发现一致。冷相和热相ICM的共存不能仅靠活动星系核（agn）的气泡上升来实现。相反，两相ICM的性质更符合cD电晕模型。在这个模型中，冷相可能归因于被限制在磁环中的等离子体，这些磁环被侵入的热相ICM包围，并被cD星系中合成的金属污染。在最内层10kpc释放的AGN反馈能量可以作为加热源，防止回路内部气体冷却到远低于观测值的温度。无论是否采用ICM温度模型，总重力质量分布都呈现分层结构。
Based on a detailed analysis of the high-quality Chandra, XMM-Newton, and Suzaku data of the X-ray bright cluster of galaxies A1795, we report clear evidence for a two-phase intracluster medium (ICM) structure, which consists of a cool (with a temperature Tc ≈ 2.0–2.2 keV) and a hot (Th ≈ 5.0–5.7 keV) component that coexist and dominate the X-ray emission at least in the central 80 kpc. A third weak emission component (T3 ≈ 0.8 keV) is also detected within the innermost 144 kpc and is ascribed to a portion of interstellar medium of the cD galaxy. Deprojected spectral analysis reveals flat radial temperature distributions for both the hot phase and cool phase components. These results are consistent with the ASCA measurements reported by Xu et al. and resemble the previous findings for the Centaurus Cluster. By analyzing the emission measure ratio and gas metal abundance maps created from the Chandra data, we find that the cool phase component is more metal-enriched than the hot phase one in the 50–100 kpc region, which agrees with that found in M87. The coexistence of the cool phase and hot phase ICM cannot be realized by bubble uplifting from active galactic nuclei (AGNs) alone. Instead, the two-phase ICM properties are better reconciled with a cD corona model. In this model, the cool phase may be ascribed to the plasmas confined in magnetic loops, which are surrounded by the intruding hot phase ICM and have been polluted by metals synthesized in the cD galaxy. AGN feedback energy released in the innermost 10 kpc can serve as the heating source to prevent the loop-interior gas from cooling down to temperatures much lower than the observed value. The total gravitating mass profile exhibits a hierarchical structure, regardless of the ICM temperature modeling.
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DOI：
10.1088/0004-637x/701/1/377
发表时间：
2009-07
期刊：
The Astrophysical Journal
影响因子：
--
作者：
I. Takahashi;M. Kawaharada;K. Makishima;K. Matsushita;Y. Fukazawa;Y. Ikebe;T. Kitaguchi;M. Kokubun;K. Nakazawa;S. Okuyama;N. Ota;T. U. O. Tokyo;Riken;Tokyo University of Science;H. University;National Museum of Emerging Science;Innovation;Japan Aerospace Exploration Agency
通讯作者：
I. Takahashi;M. Kawaharada;K. Makishima;K. Matsushita;Y. Fukazawa;Y. Ikebe;T. Kitaguchi;M. Kokubun;K. Nakazawa;S. Okuyama;N. Ota;T. U. O. Tokyo;Riken;Tokyo University of Science;H. University;National Museum of Emerging Science;Innovation;Japan Aerospace Exploration Agency
影响因子：
--
作者：
R. Fujimoto;K. Mitsuda;D. McCammon;Y. Takei;M. Bauer;Y. Ishisaki;F. Scott Porter;H. Yamaguchi;K. Hayashida;N. Yamasaki
通讯作者：
R. Fujimoto;K. Mitsuda;D. McCammon;Y. Takei;M. Bauer;Y. Ishisaki;F. Scott Porter;H. Yamaguchi;K. Hayashida;N. Yamasaki
DOI：
10.1046/j.1365-8711.1998.01478.x
发表时间：
1997-07
影响因子：
4.8
作者：
D. Buote;A. Fabian
通讯作者：
D. Buote;A. Fabian
DOI：
10.1086/321357
发表时间：
2000-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
E. Churazov;M. Brüggen;C. Kaiser;H. Böhringer;W. Forman
通讯作者：
E. Churazov;M. Brüggen;C. Kaiser;H. Böhringer;W. Forman
影响因子：
2.3
作者：
Kosuke Sato;K. Matsushita;Y. Ishisaki;N. Yamasaki;M. Ishida;S. Sasaki;T. Ohashi
通讯作者：
Kosuke Sato;K. Matsushita;Y. Ishisaki;N. Yamasaki;M. Ishida;S. Sasaki;T. Ohashi