• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >ATCA 16 cm observation of CIZA J1358.9-4750: Implication of merger stage and constraint on non-thermal properties
【24h】

ATCA 16 cm observation of CIZA J1358.9-4750: Implication of merger stage and constraint on non-thermal properties

机译：ATCA 16厘米观察CIZA J1358.9-4750：合并阶段的含义和非热性质的约束

获取原文
获取原文并翻译 | 示例
       
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

We report the Australia Telescope Compact Array 16 cm observation of CIZA J1358.9-4750. Recent X-ray studies imply that this galaxy cluster is composed of merging, binary clusters. Using the EW367 configuration, we found no significant diffuse radio emission in and around the cluster. An upper limit of the total radio power at 1.4 GHz is similar to 1.1 x 10(22) W Hz(-1) in 30 square arcminutes, which is a typical size for radio relics. It is known that an empirical relation holds between the total radio power and X-ray luminosity of the host cluster. The upper limit is about one order of magnitude lower than the power expected from the relation. Very young (similar to 70 Myr) shocks with low Mach numbers (similar to 1.3), which are often seen at an early stage of merger simulations, are suggested by the previous X-ray observation. The shocks may generate cosmic-ray electrons with a steep energy spectrum, which is consistent with non-detection of bright ( 10(23) W Hz(-1)) relic in this 16 cm band observation. Based on the assumption of energy equipartition, the upper limit gives a magnetic field strength of below 0.68f(D-los/1 Mpc)(-1)(gamma(min)/200)(-1) mu G, where f is the cosmic-ray total energy density over the cosmic-ray electron energy density, D-los is the depth of the shock wave along the sightline, and gamma(min) is the lower cutoff Lorentz factor of the cosmic-ray electron energy spectrum.
机译：我们报道了澳大利亚望远镜紧凑阵列16厘米对CIZA J1358的观测。9-4750. 最近的X射线研究表明，这个星系团由合并的双星团组成。使用EW367配置，我们发现集群内部和周围没有明显的漫反射无线电发射。1.4 GHz的总无线电功率上限类似于30平方弧分钟内的1.1 x 10（22）W Hz（-1），这是无线电文物的典型尺寸。众所周知，总射电功率与宿主星团的X射线光度之间存在经验关系。上限大约比关系中预期的幂低一个数量级。先前的X射线观测表明，在合并模拟的早期阶段经常会出现低马赫数（类似于1.3）的非常年轻（类似于70 Myr）的冲击。这些冲击可能会产生具有陡峭能谱的宇宙射线电子，这与这一16厘米波段观测中未检测到明亮（；10（23）W Hz（-1））遗迹相一致。基于能量均分的假设，上限给出的磁场强度低于0.68f（D-los/1 Mpc）（-1）（γ（min）/200）（-1）μG，其中f是宇宙线电子能量密度上的宇宙线总能量密度，D-los是激波沿视线的深度，γ（min）是宇宙线电子能谱的下限洛伦兹因子。

著录项

相似文献

  • 外文文献
  • 中文文献
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号