Study of Evolution of Galaxy Cluster and the Universe

虽然在z=0.0 - 1.0的红移范围内，k_BT-LX关系没有发现CG演化的证据，在z&lt;0.6时，k_BT-M<gas>_，k_BT-M_<Fe>，k_BT-A_<Fe>关系也没有发现CG演化的证据，但在z&gt; 0.6时，我们发现了一些演化的线索;最远的星系团AXJ 20 I9 +1127在z-1.0处的气体质量明显低于其他具有相同气体温度的CG，我们利用ASCA对M82星暴星系进行了观测，以探讨富金属离子的抛射机制气体在0.5-10 keV波段的X射线表现出薄的热谱，具有来自高度电离的镁、硅和硫的发射线，以及延伸到高于10 keV能量的硬尾。软X射线在空间上是扩展的，而硬X射线显示出一个未解决的点状结构，可能具有长期的通量变化。发射线的通量比和低能带的空间扩展结构表明 关于我们 存在至少两个温度薄热等离子体。在薄的热等离子体中的氧，氖，镁，硅，硫和铁的丰度被发现是显着低于宇宙的值。光谱的硬组分，这是空间分辨，很好地代表了吸收热韧致辐射，或吸收幂律模型。然而，硬组分的来源尚不清楚。因此，我们在1996年与ASCA进行了监测观察。虽然软组分和中等组分的X射线通量保持恒定，但在10 k s到1个月的各种时间尺度上，硬组分的X射线通量在3 &lt;<1>&gt; 10^<40>erg/s和1 &lt;<1>&gt; 10^<41>erg/s之间存在显著的时间变化。硬组分的温度或光子指数也发生了变化。我们证明了硬组分的空间位置是M82的中心。通过从最高态中减去最低态的光谱而获得的可变源的光谱表明NH- 10^ cm^的强吸收<22><-2>，这意味着可变源嵌入M82的中心。这些都表明M82中存在一个低光度活动星系核。少

Although we found no evidence of CG evolution in the k_BT-L_X relation in the redshift range of z=0.0 - 1.0, nor in the k_BT-M_<gas>, k_BT-M_<Fe>, k_BT-A_<Fe> relation in z<0.6, some hints of evolution at z>0.6 are found ; the gas masses of the most distant cluster AXJ20I9+1127 at z-1.0 are significantly lower than those of the other CGs with the same gas temperature, the iron masses of the cluster is similar to that of nearby cluster.We observed starburst galaxy M82 with ASCA in order to investigate the ejection mechanism of metal rich gas. The X-rays in the 0.5-10 keV band exhibit a thin thermal spectrum with emission lines from highly ionized magnesium, silicon, and sulfur, as well as a hard tail extending to higher than l0keV energy. The soft X-rays are spatially extended, while the hard X-rays show an unresolved point-like structure with possible a long-term flux variability. The flux ratio of the emission lines and the spatially extended structure in the low-energy band indicate … More that at least two-temperature thin thermal plasmas are present. The abundances of the oxygen, neon, magnesium, silicon, sulfur, and iron in the thin thermal plasmas are found to be significantly lower than the cosmic value.The spectrum of the hard component, which is spatially unresolved, is well represented by an absorbed thermal bremsstrahlung, or an absorbed power-law model. However the origin of the hard component was unclear. Thus, we made a monitoring observation with ASCA in 1996. Although the X-ray flux of the soft and medium components remained constant, a significant time variability of the hard component was found between 3 <<1>> 10^<40> erg/s and 1 <<1>> 10^<41> erg/s at various time scales from 10 ks to a month. The temperature or photon index of the hard component also changed. We proved that the spatial position of the hard component is the center of M82. The spectrum of the variable source obtained by subtracting the spectrum of the lowest state from the highest state suggests the strong absorption of NH- 10^<22> cm^<-2>, which means the variable source is embedded in the center of M82. All these suggest that a low-luminosity AGN exists in M82. Less