星系团中的吸积激波及其SZ特征的宇宙学模拟
Accretion Shocks in Clusters of Galaxies and their SZ Signature from Cosmological Simulations
摘要：
冷暗物质（CDM）分级结构形成模型预测存在大规模吸积冲击的维里和周转半径的星系团。Kocsis等人（2005年）认为，与这种冲击相关的Sunyaev-Zel'dovich（SZ）信号可能会被下一代射电干涉仪ALMA观测到。利用自适应网格加密（AMR）和光滑粒子流体动力学（SPH）方法对暗能量主导的CDM（LCDM）模型进行模拟，研究了星系团周围吸积激波的三维分布.在松弛的集群中，我们发现两组不同的冲击。一组（“维里激波”），马赫数为2.5-4，位于半径为0.9-1.3 Rvir处，其中Rvir是对维里半径的球面估计，覆盖了这些半径处星系团周围总表面积的40-50%。另一组较强的激波（“外部激波”）位于更远的地方，大约3 Rvir，具有大的马赫数（~100），覆盖大约40-60%的表面积。我们模拟了由高分辨率AMR运行绘制的弛豫大质量星系团的SZ表面亮度图，并得出ALMA应该能够探测大质量星系团中的维里激波的结论。需要进行更多的模拟，以改进对天体物理噪声的估计，并确定最佳观测策略。
英文摘要：
Cold dark matter (CDM) hierarchical structure formation models predict the existence of large-scale accretion shocks between the virial and turnaround radii of clusters of galaxies. Kocsis et al. (2005) suggest that the Sunyaev-Zel'dovich (SZ) signal associated with such shocks might be observable with the next generation radio interferometer, ALMA. We study the three--dimensional distribution of accretion shocks around individual clusters of galaxies drawn from adaptive mesh refinement (AMR) and smoothed particle hydrodynamics (SPH) simulations of LCDM (dark energy dominated CDM) models. In relaxed clusters, we find two distinct sets of shocks. One set ("virial shocks"), with Mach numbers of 2.5-4, is located at radii 0.9-1.3 Rvir, where Rvir is the spherical infall estimate of the virial radius, covering about 40-50% of the total surface area around clusters at these radii. Another set of stronger shocks ("external shocks") is located farther out, at about 3 Rvir, with large Mach numbers (~100), covering about 40-60% of the surface area. We simulate SZ surface brightness maps of relaxed massive galaxy clusters drawn from high resolution AMR runs, and conclude that ALMA should be capable of detecting the virial shocks in massive clusters of galaxies. More simulations are needed to improve estimates of astrophysical noise and to determine optimal observational strategies.
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