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-L_X关系中没有发现CG演化的证据，在z&gt；0.6的k_BT-M_&lt；GAs&gt；，k_BT-M_&lt；Fe&gt；，k_BT-A_&lt；Fe&gt；关系中也没有发现CG演化的证据，但在z&gt；0.6处发现了一些演化的迹象；在z-1.0时，最远的星系团AXJ20I9+1127的气体质量明显低于相同气体温度下的其他星系团，该星系团的铁质量与附近星系团的铁质量相近。为了研究富金属气体的抛射机制，我们用ASCA观测了星暴星系M82。0.5-10keV波段的X射线表现出很薄的热谱，有高度电离的镁、硅和硫的发射线，以及延伸到高于10keV能量的硬尾巴。软X射线在空间上是延伸的，而硬X射线则表现出一种可能具有长期通量变异性的未分辨的点状结构。发射线的通量比和低能带中的空间扩展结构指示…更重要的是，至少存在两个温度较薄的热等离子体。薄的热等离子体中的氧、霓虹灯、镁、硅、硫和铁的丰度明显低于宇宙值。硬成分的光谱在空间上没有分辨，很好地用吸收的热韧致辐射或吸收的幂定律模型来表示。然而，硬部件的来源尚不清楚。因此，我们在1996年与ASCA进行了一次监测观测。尽管软组分和中组分的X射线通量保持不变，但在10k至1个月的不同时间尺度上，3&lt；1&gt；1&gt；40&gt；3&lt；1&gt；40&gt；S和1&lt；1&gt；10&gt；41&gt；erg/S之间发现了显著的时间变异性。硬部件的温度或光子指数也发生了变化。我们证明了硬部件的空间位置是M82的中心。从最高态减去最低态的光谱得到的可变源的光谱表明NH-10^&lt；22&gt；Cm^&lt；-2&gt；有很强的吸收，这意味着可变源嵌入在M82的中心。所有这些都表明，M82中存在一个低光度活动星系核。较少

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