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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 with a radio relic
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Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 with a radio relic

机译：Suzaku和Chandra的Galaxy Cluster RXC J1053.7 + 5453与无线电遗物的观察

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We present the results of Suzaku and Chandra observations of the galaxy cluster RXC J1053.7+5453 (z = 0.0704), which contains a radio relic. The radio relic is located at a distance of similar to 540 kpc from the X-ray peak toward the west. We measured the temperature of this cluster for the first time. The resultant temperature in the center is similar to 1.3 keV, which is lower than the value expected from the X-ray luminosity-temperature and the velocity dispersion-temperature relations. Though we did not find a significant temperature jump at the outer edge of the relic, our results suggest that the temperature decreases outward across the relic. Assuming the existence of the shock at the relic, its Mach number becomes M similar or equal to 1.4. A possible spatial variation of Mach number along the relic is suggested. Additionally, a sharp surface brightness edge is found at a distance of similar to 160 kpc from the X-ray peak toward the west in the Chandra image. We performed X-ray spectral and surface brightness analyses around the edge with the Suzaku and Chandra data, respectively. The obtained surface brightness and temperature profiles suggest that this edge is not a shock but likely a cold front. Alternatively, it cannot be ruled out that thermal pressure is really discontinuous across the edge. In this case, if the pressure across the surface brightness edge is in equilibrium, other forms of pressure sources, such as cosmic-rays, are necessary. We searched for the non-thermal inverse Compton component in the relic region. Assuming a photon index Gamma = 2.0, the resultant upper limit of the flux is 1.9 x 10(-14) erg s(-1) cm(-2) for a 4.50 x 10(-3) deg(2) area in the 0.3-10 keV band, which implies that the lower limit of magnetic field strength becomes 0.7 mu G.
机译：我们介绍了舒萨库和Chandra的结果，银河群RXC J1053.7 + 5453（Z = 0.0704），其中包含无线电遗物。无线电遗物位于与朝向西部的X射线峰值类似于540kPc的距离。我们首次测量了该簇的温度。中心的所得温度类似于1.3keV，低于X射线光度 - 温度和速度分散温度关系的预期值。虽然我们在遗物的外边上没有发现显着的温度跳跃，但我们的结果表明温度在遗物上向外降低。假设遗物处的冲击的存在，其马赫数变为M类似或等于1.4。建议沿着遗物的可能空间变化。另外，在Chandra图像中，从X射线峰值与X射线峰值相似的距离相似的尖锐表面亮度边缘。我们分别在边缘和Chandra数据周围进行了X射线光谱和表面亮度分析。所获得的表面亮度和温度曲线表明，该边缘不是震荡，但可能是一个冷的前沿。或者，不能排除热压在边缘中真正不连续。在这种情况下，如果表面亮度边缘的压力处于平衡，则需要其他形式的压力源，例如宇宙射线。我们在遗物区域中搜索了非热反转康普顿组件。假设光子指数伽马= 2.0，所得通量的上限为1.9×10（-14）厘米（-1）cm（-2），用于4.50×10（-3）°（2）区域0.3-10 kev频段，这意味着磁场强度的下限变为0.7μg。

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