Euclid筹备工作。XLII. 对五项成像巡天中星系团弱引力透镜的统一星表级再分析
Euclid preparation. XLII. A unified catalogue-level reanalysis of weak lensing by galaxy clusters in five imaging surveys
AI总结：
本研究利用Euclid的COMB-CL管线对五项独立透镜巡天数据开展统一星表级分析，验证了星系团弱引力透镜质量测量的系统误差控制效果，为Euclid阶段大样本星系团质量测量奠定了基础。
摘要：
在Euclid时代，要将星系团用作天体物理和宇宙学探针，需要精确且准确的质量定标。通过比较具有独立且不相关系统误差的不同巡天，可以凭经验估算星系团透镜信号中的系统误差。为评估透镜结果对系统误差的稳健性，我们在不同数据集间开展了端到端测试。我们利用Euclid星系团与弱引力透镜联合管线（COMB-CL）在星表层面进行了统一分析，COMB-CL将用于Euclid巡天的弱引力透镜星系团质量测量。我们在相同的模型假设下，采用一致的管线分析了来自五项独立近期透镜巡天（CHFTLenS、DES SV1、HSC-SSP S16a、KiDS DR4和RCSLenS）的异质数据集，这些巡天采用了不同的剪切和测光红移估计算法。我们使用Planck PSZ2和SDSS redMaPPer星系团样本作为透镜，对比了约化面密度超额的幅度以及质量估计值。所得质量估计与LC2星表中收录的文献结果一致。我们还通过HSC-SSP XXL北天区中AMICO探测到的星系团，进一步研究了质量精度。我们利用统一分析框架测试了数据集的一致性，发现各独立巡天之间的结果吻合度处于第三阶段（Stage-III）巡天或先导巡天的系统噪声水平，这表明系统误差得到了成功控制。若第四阶段（Stage-IV）巡天能保持这种控制水平，Euclid将能够测量约13000个（仅考虑散粒噪声）或3000个（考虑形状和大尺度结构噪声）大质量星系团的弱引力透镜质量，且信噪比大于3。
英文摘要：
Precise and accurate mass calibration is required to exploit galaxy clusters as astrophysical and cosmological probes in the Euclid era. Systematic errors in lensing signals by galaxy clusters can be empirically estimated by comparing different surveys with independent and uncorrelated systematics. To assess the robustness of the lensing results to systematic errors, we carried out end-to-end tests across different data sets. We performed a unified analysis at the catalogue level by leveraging the Euclid combined cluster and weak-lensing pipeline (COMB-CL). COMB-CL will measure weak lensing cluster masses for the Euclid Survey. Heterogeneous data sets from five independent, recent, lensing surveys (CHFTLenS, DES~SV1, HSC-SSP~S16a, KiDS~DR4, and RCSLenS), which exploited different shear and photometric redshift estimation algorithms, were analysed with a consistent pipeline under the same model assumptions. We performed a comparison of the amplitude of the reduced excess surface density and of the mass estimates using lenses from the Planck PSZ2 and SDSS redMaPPer cluster samples. Mass estimates agree with literature results collected in the LC2 catalogues. Mass accuracy was further investigated considering the AMICO detected clusters in the HSC-SSP XXL North field. The consistency of the data sets was tested using our unified analysis framework. We found agreement between independent surveys, at the level of systematic noise in Stage-III surveys or precursors. This indicates successful control over systematics. If such control continues in Stage-IV, Euclid will be able to measure the weak lensing masses of around 13000 (considering shot noise only) or 3000 (noise from shape and large-scale-structure) massive clusters with a signal-to-noise ratio greater than 3.
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