A. Paliwal, W. Cui, D. D. Andr'es, M. Petris, A. Ferragamo, C. Hanser, J. Macı́as-Pérez, F. Mayet, A. Moyer-Anin, M. Muñoz-Echeverría, L. Perotto, E. Rasia, G. Yepes
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引用次数: 0
摘要
星系团的质量和红移丰度是一个众所周知的宇宙学探测指标。星系团质量是利用星系团约束宇宙学参数研究的一个关键参数,因此了解并正确解释其估算误差至关重要。因此,正确校准康普顿综合参数等观测指标与星系团质量之间的比例关系就变得非常重要。通过 NIKA2 Sunyaev-Zeldovich Large 程序(LPSZ),我们可以在毫米波长波段绘制出非常详细的星团内介质剖面图(在 1.2 和 2 毫米波长波段的分辨率分别为 11 和 17″),从而比以前的 SZ 观测更精确地估算出星团的静水质量。然而,某些系统性影响只能通过模拟来解释。为此,我们采用了 "The Three Hundred "模拟,这些模拟使用了一系列物理模块来模拟星系团。所谓的孪生样本是通过选取与 LPSZ 观测目标性质相近的合成星系团来构建的。我们特别使用了这些孪生样本沿29条不同视线的康普顿参数图和投影总质量图。我们研究了投影对总质量的影响。最后,我们考虑了沿不同视线的统计值,在综合康普顿参数、总质量和星系团的过密度之间构建了一种三维比例定律,以确定受投影效应影响最小的过密度。
3D scaling laws and projection effects in The300-NIKA2 Sunyaev-Zeldovich Large Program Twin Samples
The abundance of galaxy clusters with mass and redshift is a wellknown cosmological probe. The cluster mass is a key parameter for studies that aim to constrain cosmological parameters using galaxy clusters, making it critical to understand and properly account for the errors in its estimates. Subsequently, it becomes important to correctly calibrate scaling relations between observables like the integrated Compton parameter and the mass of the cluster. The NIKA2 Sunyaev-Zeldovich Large program (LPSZ) enables one to map the intracluster medium profiles in the mm–wavelength band with great details (resolution of 11 & 17″ at 1.2 & 2 mm, respectively) and hence, to estimate the cluster hydrostatic mass more precisely than previous SZ observations. However, there are certain systematic effects which can only be accounted for with the use of simulations. For this purpose, we employ The Three Hundred simulations which have been modelled with a range of physics modules to simulate galaxy clusters. The so-called twin samples are constructed by picking synthetic clusters of galaxies with properties close to the observational targets of the LPSZ. In particular, we use the Compton parameter maps and projected total mass maps of these twin samples along 29 different lines of sight. We investigate the scatter that projection induces on the total masses. Eventually, we consider the statistical values along different lines of sight to construct a kind of 3D scaling law between the integrated Compton parameter, total mass, and overdensity of the galaxy clusters to determine the overdensity that is least impacted by the projection effect.