We applied a scientific approach to the problem of the effective area cross-calibration of the XMM-Newton EPIC instruments. Using a sample of galaxy clusters observed with the XMM-Newton EPIC, we quantified the effective area cross-calibration bias between the EPIC instruments as implemented in the public calibration data base on November 2021 in the 0.5-6.1 keV energy band. We invested significant efforts in controlling and minimising the systematic uncertainties of the cross-calibration bias below 1%. The statistical uncertainties are similar and thus we can reliably measure effects at 1% level. The effective area cross-calibration in the 0.5-6.1 keV band between MOS and pn is biased at a substantial level. The MOS/pn bias is systematic suggesting that MOS (pn) effective area may be calibrated too low (high), by $\sim$3-27% on average depending on the instrument and energy band. The excellent agreement of the energy dependencies (i.e. shapes) of the effective area of MOS2 and pn suggest that they are correctly calibrated within $\sim$1% in the 0.5-4.5 keV band. Comparison with an independent data set of point sources (3XMM) confirms this. The cluster sample indicates that the MOS1/pn effective area shape cross-calibration has an approximately linear bias amounting to $\sim$10% in maximum in the 0.5-4.5 keV band. The effective area cross-calibration of XMM-Newton/EPIC instruments on November 2021 in the 0.5-4.5 keV band is in a relatively good shape. However, the cluster-to-cluster rms scatter of the bias is substantial compared to the median bias itself. Thus, a statistically robust implementation of the cross-calibration uncertainties to a scientific analysis of XMM-Newton/EPIC data should include the propagation of the scatter to the best-fit parameters, instead of a simple average bias correction of the effective area.
Multichroic TES Bolometers and Galaxy Cluster Mass Scaling Relations with the South Pole Telescope
南极望远镜（英语：South Pole Telescope）是一个高分辨率的微波频率望远镜，用于观测宇宙微波背景（CMB）。到目前为止，已经在SPT上安装了两台摄像机，对CMB进行了两次调查，第一次是强度调查（SPT-SZ），第二次是强度和偏振调查（SPTpol）。目前正在开发第三代偏振敏感相机（SPT-3G）。本论文介绍了工作跨越所有三个仪器上的SPT。我提出我的工作在时间颠倒的顺序，遵循仪器开发，部署和分析的规范叙述。首先，新的3波段多色过渡边缘传感器（TES）的SPT-3G实验测辐射热计的开发和测试进行了详细说明，其次是频率复用低温读出电子的SPTpol实验的开发和部署，并得出结论与SPT-SZ仪器所采取的数据分析。我描述了一个贝叶斯似然为基础的方法，我开发的测量综合康普顿化（YSZ）的星系团的Sunyaev-Zel 'dovich（SZ）效应，并限制星系团YSZ质量标度关系的发展。
