探测团簇芯中的类声波表面亮度波动
Detecting Sound-Wave-Like Surface Brightness Ripples in Cluster Cores
摘要：
我们调查的观测要求检测声波样功能的星系团的核心。我们计算了投影对观测到的波振幅的影响，发现投影因子仅弱地依赖于基本的集群属性，但强烈地依赖于声波的波长，与观测到的振幅被减少了一个因素~5为5 kpc波，但只有一个因素~ 2为25 kpc波。我们继续估计所需的时间来检测类似于以前在英仙座集群中检测到的涟漪在其他集群。我们发现，检测时间尺度最强烈的集群的通量和波纹的幅度。通过连接的纹波振幅的加热功率的系统中，我们估计检测时间选择的本地集群，并发现几个可能有纹波检测到的~ 1 Ms钱德拉时间。
英文摘要：
We investigate the observational requirements for the detection of sound-wave-like features in galaxy cluster cores. We calculate the effect of projection on the observed wave amplitude, and find that the projection factor depends only weakly on the underlying cluster properties but strongly on the wavelength of the sound waves, with the observed amplitude being reduced by a factor ~5 for 5 kpc waves but only by a factor ~ 2 for 25 kpc waves. We go on to estimate the time needed to detect ripples similar to those previously detected in the Perseus cluster in other clusters. We find that the detection time scales most strongly with the flux of the cluster and the amplitude of the ripples. By connecting the ripple amplitude to the heating power in the system, we estimate detection times for a selection of local clusters and find that several may have ripples detected with ~1Ms Chandra time.
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。
