An XMM-Newton study of the RGH 80 galaxy group
An XMM-Newton study of the RGH 80 galaxy group
复制标题
DOI：
10.1051/0004-6361:20035760
复制
发表时间：
2004-03
影响因子：
6.5
通讯作者：
Yan-jie Xue;H. Böhringer;K. Matsushita
中科院分区：
文献类型：
--
作者：
Yan-jie Xue;H. Böhringer;K. Matsushita
我们给出了XMM-牛顿观测到的RGH-80星系团的X射线研究。气体的X射线发射被探测到∼462h−150kpc，对应于∼0.45r200。该群的温度为1.01±0.01keV，气体相对丰富，发光。用去投影谱分析发现，温度峰值在0.11r200附近的∼1.3k eV处，然后在中心处向内减小到0.83keV，在大半径处向外减小到∼峰值的70%。在气体冷却时间小于哈勃时间组的中心∼60kpc内，温度为0.82keV和1.51keV，银河吸收的双温模型给出了最好的光谱拟合，其中冷组分占∼体积的20%。我们还得到了气体的熵分布，与冷却和/或内部加热模型的预测是一致的。此外，氧、镁、硅、S和铁的丰度随着半径的增大而单调下降。根据观测到的丰度比模式，我们估计∼85%或∼72%的铁质量是由SN Ia贡献的，这取决于所采用的SN II模型。
We present an X-ray study of the galaxy group RGH 80, observed by XMM-Newton. The X-ray emission of the gas is detected out to ∼462 h −1 50 kpc, corresponding to ∼0.45r200. The group is relatively gas rich and luminous with respect to its temperature of 1.01 ± 0.01 keV. Using the deprojected spectral analysis, we find that the temperature peaks at ∼1. 3k eV around 0.11r200, and then decreases inwards to 0.83 keV at the center and outwards to ∼70% of the peak value at large radii. Within the central ∼60 kpc of the group where the gas cooling time is less than the Hubble time, a two-temperature model with temperatures of 0.82 and 1.51 keV and the Galactic absorption gives the best fit of the spectra, with ∼20% volume occupied by the cool component. We also derive the gas entropy distribution, which is consistent with the prediction of cooling and/or internal heating models. Furthermore, the abundances of O, Mg, Si, S and Fe decrease monotonically with radius. With the observed abundance ratio pattern, we estimate that ∼85% or ∼72% of the iron mass is contributed by SN Ia, depending on the adopted SN II models.