The large-scale shock in the cluster of galaxies Hydra A
The large-scale shock in the cluster of galaxies Hydra A
复制标题
长蛇座 A 星系团的大规模激波
DOI：
10.1051/0004-6361:200811071
复制
发表时间：
2009
影响因子：
6.5
通讯作者：
Finoguenov
中科院分区：
文献类型：
--
作者：
Simionescu;Roediger;Nulsen;P. E. J;Brüggen;Forman;Böhringer;H.Werner;Finoguenov
我们分析了对Hydra A星系团的深度XMM-牛顿观测，重点是钱德拉图像中发现的大规模冲击，作为表面亮度的不连续性。在压力图和几个扇区的温度分布图中都可以看到激波阵面。我们比较了一个球对称的流体动力学模型的结果，表面亮度分布和温度跳跃的冲击，以确定冲击的属性。由温度跃变确定的马赫数与由EPIC/pn表面亮度廓线和以前由Chandra数据得到的马赫数很好地一致，并且与M ~ 1.3一致。在这个简单的模型中，估计的冲击年龄在不同的部门之间的范围在1.3亿和2.3亿年之间的爆发能量在1.5和31061 erg。在压力图中看到的激波形状可以近似为一个椭圆，中心约为70 kpc，从星团中心向东北方向移动。这是一个很好的简单近似的冲击波形状看到钱德拉图像，虽然这个形状显示出额外的小偏差椭圆。我们的目标是发展一个更好的模型，可以解释的激波中心和活动星系核之间的偏移，以及给出一个一致的结果，对激波的年龄和能量。为此，我们进行了三维流体动力学模拟，其中的冲击是由一对对称的活动星系核喷流发射在一个球形星系团。为了解释观测到的激波中心和活动星系核之间的偏移，我们考虑了模拟中包含的团内介质中的大规模整体流动。模拟成功地再现了所观察到的激波阵面的大小、椭圆率和平均马赫数。预测的冲击年龄为1.6亿年，总输入能量为31061 erg。这两个值都在球对称模型确定的范围内。为了通过大尺度相干运动来匹配观测到的激波椭圆距星团中心70 kpc的偏移量，这些运动需要具有670 km s-1的高速度。我们讨论了这种情况下的可行性，并提供替代方法来产生观察到的偏移，并进一步改善模拟。
We analyzed a deep XMM-Newton observation of the cluster of galaxies Hydra A, focusing on the large-scale shock discovered in Chandra images as a discontinuity in the surface brightness. The shock front can be seen both in the pressure map and in temperature profiles in several sectors. We compared the results of a spherically symmetric hydrodynamic model to surface brightness profiles and temperature jumps across the shock to determine the shock properties. The Mach numbers determined from the temperature jumps are in good agreement with the Mach numbers derived from EPIC/pn surface brightness profiles and previously from Chandra data and are consistent withM~ 1.3. In this simple model, the estimated shock age in the different sectors ranges between 130 and 230 Myr and the outburst energy between 1.5 and 3 1061erg. The shape of the shock seen in the pressure map can be approximated with an ellipse centered ~70 kpc towards the NE from the cluster center. This is a good simple approximation to the shock shape seen in the Chandra image, although this shape shows additional small deviations from ellipticity. We aimed to develop a better model that can explain the offset between the shock center and the AGN, as well as give a consistent result on the shock age and energy. To this end, we performed 3D hydrodynamical simulations in which the shock is produced by a symmetrical pair of AGN jets launched in a spherical galaxy cluster. As an explanation of the observed offset between the shock center and the AGN, we consider large-scale bulk flows in the intracluster medium, which were included in the simulation. The simulation successfully reproduces the size, ellipticity, and average Mach number of the observed shock front. The predicted age of the shock is 160 Myr and the total input energy 3 1061erg. Both values are within the range determined by the spherically symmetric model. To match the observed 70 kpc offset of the shock ellipse from the cluster center by large-scale coherent motions, these would need to have a high velocity of 670 km s-1. We discuss the feasibility of this scenario and offer alternative ways to produce the observed offset and to further improve the simulation.
登录
查看更多内容
DOI：
10.1111/j.1745-3933.2007.00351.x
发表时间：
2007-06
影响因子：
--
作者：
M. Brueggen;S. Heinz;E. Roediger;M. Ruszkowski;A. Simionescu
通讯作者：
M. Brueggen;S. Heinz;E. Roediger;M. Ruszkowski;A. Simionescu
使用 XMM-Newton 观察到的 A1413 的质量分布：对 M-T 关系的影响
DOI：
--
发表时间：
2002
期刊：
影响因子：
--
作者：
G. Pratt;M. Arnaud
通讯作者：
M. Arnaud
DOI：
10.1086/591228
发表时间：
2008-06
期刊：
The Astrophysical Journal
影响因子：
--
作者：
E. Scannapieco;M. Brüggen
通讯作者：
E. Scannapieco;M. Brüggen
DOI：
10.1111/j.1745-3933.2006.00243.x
发表时间：
2006-06
影响因子：
--
作者：
S. Heinz;S. Heinz;M. Brüggen;A. Young;Emily M. Levesque
通讯作者：
S. Heinz;S. Heinz;M. Brüggen;A. Young;Emily M. Levesque
影响因子：
6.5
作者：
N. Werner;J. Plaa;J. Plaa;J. Kaastra;J. Vink;J. Vink;J. Bleeker;J. Bleeker;T. Tamura;J. Peterson;F. Verbunt
通讯作者：
N. Werner;J. Plaa;J. Plaa;J. Kaastra;J. Vink;J. Vink;J. Bleeker;J. Bleeker;T. Tamura;J. Peterson;F. Verbunt