The X-ray luminous cluster underlying the z = 1.04 quasar PKS 1229−021
The X-ray luminous cluster underlying the z = 1.04 quasar PKS 1229−021
复制标题
z = 1.04 类星体 PKS 1229−021 下方的 X 射线发光星团
DOI：
--
复制
发表时间：
2012
期刊：
影响因子：
--
通讯作者：
E. Belsole
中科院分区：
文献类型：
--
作者：
H. Russell;A. Fabian;G. Taylor;J. Sanders;K. Blundell;C. Crawford;R. Johnstone;E. Belsole
我们提出了一个100ks钱德拉观测，研究了强大的类星体PKS 1229−021周围z= 1.04的扩展x射线发射。弥漫性星团x射线辐射可以追踪到~ 15弧秒（~ 120 kpc）半径，并且在中心5弧秒内计算出的硬度比下降，这与冷核的存在一致。对这颗类星体的射电观测显示，它有一个强大的核心，一个明亮的单侧喷流通往西南热点，在反喷流一侧可见第二个热点。尽管类星体点扩展函数（PSF）的翼对探测到扩展星团发射的所有半径处的总x射线通量有重要贡献，但我们能够使用钱德拉射线追踪器和马克思模拟准确地减去PSF发射。由此得出的PKS 1229−021星团表面亮度曲线与FR II （Fanaroff-Riley类II）射电星系3C 444的曲线相似，后者的表面亮度也因射电叶周围的强烈冲击而迅速下降。利用基于3C 444的模型表面亮度剖面，我们估计了PKS 1229−021的总光度为。我们讨论了在高红移巡天中探测拥有明亮x射线源的冷核星团的困难。
We present a 100 ks Chandra observation studying the extended X-ray emission around the powerful z= 1.04 quasar PKS 1229−021. The diffuse cluster X-ray emission can be traced out to ∼15 arcsec (∼120 kpc) radius and there is a drop in the calculated hardness ratio inside the central 5 arcsec consistent with the presence of a cool core. Radio observations of the quasar show a strong core and a bright, one-sided jet leading to the south-west hotspot and a second hotspot visible on the counter-jet side. Although the wings of the quasar point spread function (PSF) provided a significant contribution to the total X-ray flux at all radii where the extended cluster emission was detected, we were able to accurately subtract the PSF emission using Chandra Ray Tracer and marx simulations. The resulting steep cluster surface brightness profile for PKS 1229−021 appears similar to the profile for the FR II (Fanaroff–Riley class II) radio galaxy 3C 444, which has a similarly rapid surface brightness drop caused by a powerful shock surrounding the radio lobes. Using a model surface brightness profile based on 3C 444, we estimated the total cluster luminosity for PKS 1229−021 to be . We discuss the difficulty of detecting cool-core clusters, which host bright X-ray sources, in high redshift surveys.
DOI：
10.1088/0004-637x/745/1/84
发表时间：
2011-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
B. Wilkes;D. Lal;D. M. Worrall;M. Birkinshaw;M. Haas;S. Willner;R. Antonucci;M. Ashby;M. Avara;P. Barthel;R. Chini;R. Chini;Giovanni Fazio;M. Hardcastle;C. R. Lawrence;C. Leipski;P. Ogle;B. Schulz
通讯作者：
B. Wilkes;D. Lal;D. M. Worrall;M. Birkinshaw;M. Haas;S. Willner;R. Antonucci;M. Ashby;M. Avara;P. Barthel;R. Chini;R. Chini;Giovanni Fazio;M. Hardcastle;C. R. Lawrence;C. Leipski;P. Ogle;B. Schulz