Chandra observations of Abell 2199
Chandra observations of Abell 2199
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DOI：
10.1046/j.1365-8711.2002.05743.x
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发表时间：
2002-02
影响因子：
4.8
通讯作者：
R. Johnstone;S. Allen;A. Fabian;J. Sanders
中科院分区：
文献类型：
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作者：
R. Johnstone;S. Allen;A. Fabian;J. Sanders
我们目前的结果从两个钱德拉观测的丰富，附近的星系团阿贝尔2199的分析。我们发现的证据（已校正投影效应）的径向梯度的温度和金属量的X射线发射气体：温度下降从kT 4.2 keV在R = 200 kpc的1.6 keV内R = 5 kpc的中心。金属丰度从R = 200 kpc时的0.3太阳能上升到R = 30 kpc时的0.7太阳能，然后在中央5 kpc内下降到0.3太阳能。我们发现的证据与中央射电源3C 338的表面亮度分布的结构。没有证据表明，在任何特定的位置，尽管冷却时间很短（<10 - 9年），在中央15 kpc的气体有一个大的温度分布。加热和质量冷却速率计算各种假设的状态的气体。
We present results from an analysis of two Chandra observations of the rich, nearby galaxy cluster Abell 2199. We find evidence (having corrected for projection effects) for radial gradients in temperature and metallicity in the X-ray emitting gas: the temperature drops from kT ∼ 4.2 keV at R = 200 kpc to 1.6 keV within R = 5 kpc of the centre. The metallicity rises from ∼0.3 solar at R = 200 kpc to ∼0.7 solar at R = 30 kpc before dropping to 0.3 solar within the central 5 kpc. We find evidence for structure in the surface brightness distribution associated with the central radio source 3C 338. No evidence is found for the gas having a large spread in temperature at any particular location despite the cooling time being short (<10 9 yr) within the central ∼15 kpc. Heating and mass cooling rates are calculated for various assumptions about the state of the gas.