对英仙座星系团核心的更深入X射线研究：声波的功率以及金属和宇宙射线的分布
A deeper X-ray study of the core of the Perseus galaxy cluster: the power of sound waves and the distribution of metals and cosmic rays
摘要：
进一步研究了英仙座X射线最亮的星系团A426的超深Chandra观测。我们研究的径向分布推断的准同心波纹表面亮度的能量通量，假设它们是由于声波，并表明，这是一个显着的部分内75-100千秒差距，其中的冷却时间是4-5 Gyr，分别由辐射冷却损失的能量。波通量随半径向外减小，与能量耗散一致。一些新发现的超过100 kpc的大波纹，以及一个可能在170 kpc半径的完整气泡，可能表明原子核在几百万年前有过更高水平的活动。金属在团内气体中的分布在半径约40 kpc处达到峰值，在5 kpc尺度上明显呈聚集性。详细分析了在50 kpc内发现的软X射线灯丝和硬X射线发射成分的温度分布。由非热电子产生的压力，导致了被解释为逆康普顿发射的光谱分量，在中心40千秒差距内很高，并提高了那里的声波的功率;超过40千秒差距，它急剧下降。我们没有发现来自射电泡的热辐射;为了使任何热气体在泡内具有超过50%的填充因子，该气体的温度必须超过50 keV。
英文摘要：
We make a further study of the very deep Chandra observation of the X-ray brightest galaxy cluster, A426 in Perseus. We examine the radial distribution of energy flux inferred by the quasi-concentric ripples in surface brightness, assuming they are due to sound waves, and show that it is a significant fraction of the energy lost by radiative cooling within the inner 75-100 kpc, where the cooling time is 4-5 Gyr, respectively. The wave flux decreases outward with radius, consistent with energy being dissipated. Some newly discovered large ripples beyond 100 kpc, and a possible intact bubble at 170 kpc radius, may indicate a larger level of activity by the nucleus a few 100 Myr ago. The distribution of metals in the intracluster gas peaks at a radius of about 40 kpc and is significantly clumpy on scales of 5 kpc. The temperature distribution of the soft X-ray filaments and the hard X-ray emission component found within the inner 50 kpc are analysed in detail. The pressure due to the nonthermal electrons, responsible for a spectral component interpreted as inverse Compton emission, is high within 40 kpc of the centre and boosts the power in sound waves there; it drops steeply beyond 40 kpc. We find no thermal emission from the radio bubbles; in order for any thermal gas to have a filling factor within the bubbles exceeding 50 per cent, the temperature of that gas has to exceed 50 keV.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
