Correlation of the magnetic field and the intra-cluster gas density in galaxy clusters
Correlation of the magnetic field and the intra-cluster gas density in galaxy clusters
复制标题
星系团中磁场与团内气体密度的相关性
DOI：
10.1051/0004-6361:20011219
复制
发表时间：
2001
影响因子：
6.5
通讯作者：
L. Feretti
中科院分区：
文献类型：
--
作者：
K. Dolag;S. Schindler;F. Govoni;L. Feretti
我们提出了星系团中X射线表面亮度和法拉第旋转测量之间的关联，这一关联既来自射电和X射线观测，也来自星系团内介质的建模。观察到的关联排除了在整个星系团中具有恒定强度的磁场。对星系团的宇宙学、磁流体动力学模拟表明，对于宇宙起源的磁场来说，这种关联是预期的，并很好地再现了观测结果，表明法拉第旋转的均方根散射随X射线表面亮度线性增加。从观测到的量子数、旋转量和X射线表面亮度之间的关系，我们推断出物理量：磁场强度和气体密度之间的关系。对于现有的最佳观测，即A119的观测，我们认为B/N为0：9 E。
We present a correlation between X-ray surface brightness and Faraday rotation measure in galaxy clusters, both, from radio and X-ray observations as well as from modeling of the intra-cluster medium. The ob- served correlation rules out a magnetic eld of constant strength throughout the cluster. Cosmological, magneto- hydrodynamic simulations of galaxy clusters are used to show that for a magnetic eld of cosmic origin this correlation is expected and excellently reproduces the observations showing that the rms scatter of the Faraday rotation increases linearly with the X-ray surface brightness. From the correlation between the observable quanti- ties, rotation measure and X-ray surface brightness, we infer a relation between the physical quantities: magnetic eld and gas density. For the best available observations, those of A119, we nd B/ n 0:9 e .