photo-3x2-pt：利用单个测光星系目录开展宇宙剪切与星系成团的宇宙学研究
photo-3x2-pt: Cosmology from cosmic shear and galaxy clustering with a single photometric galaxy catalog
AI总结：
该研究基于 HSC-Y3 数据，采用 photo-3x2-pt 方法开展联合宇宙学分析，得到精度提升约 25%的 $S_8$ 约束，且通过模拟验证了分析的可靠性。
AI中文摘要：
我们利用从 Hyper Suprime-Cam 第 3 年（HSC-Y3）弱引力透镜形状目录中测量得到的星系成团角功率谱、星系-剪切交叉关联以及宇宙剪切（以下统称为 photo-3x2-pt）进行联合宇宙学分析。我们采用伪 $C_\ell$ 方法测量这些功率谱，并运用模板去投影方法降低星系密度图中的系统误差。我们基于测量得到的 photo-3x2-pt 开展标准贝叶斯似然分析以进行宇宙学推断，其中包含了星系内禀对齐、星系成团偏差、引力透镜放大效应、重子反馈效应以及源红移分布误差的贡献。对于平坦冷暗物质模型，我们得到 $0.76 \le S_8 \le 0.81$ 的 68%可信区间。该结果与 HSC-Y3 宇宙剪切分析（Dalal 等人 2023，Li 等人 2023）的结果一致，但比其精度高约 25%。我们还使用模拟 HSC-Y3 数据的模拟目录进行性能测试，以验证我们的 photo-3x2-pt 分析。通过对模拟数据进行贝叶斯参数推断，我们验证了可以得到关键宇宙学和冗余参数的无偏估计，包括 $S_8$、内禀对齐的模型参数、星系成团偏差以及源红移分布的偏移参数。
英文摘要：
We perform a joint cosmological analysis using angular power spectra of galaxy clustering, galaxy-shear cross correlation, and cosmic shear (hereafter referred to as photo-3x2-pt) measured from the Hyper Suprime-Cam year-3 (HSC-Y3) weak lensing shape catalog. We employ the pseudo-$C_\ell$ method to measure these power spectra and use the template deprojection method to mitigate systematics in the galaxy density maps. We perform a standard Bayesian likelihood analysis for cosmological inference based on the measured photo-3x2-pt, including contributions from intrinsic alignments of galaxies, galaxy clustering bias, lensing magnification effect, baryonic feedback effect, and source redshift distribution errors. For a flat cold dark matter model, we find a 68% credible interval of $0.76 \le S_8 \le 0.81$. This result is consistent with those of the HSC-Y3 cosmic shear analyses (Dalal et al. 2023, Li et al. 2023), but is $\sim 25$% tighter than theirs. We also perform a performance test using mock catalogs that mimic the HSC-Y3 data to validate our photo-3x2-pt analysis. Through Bayesian parameter inference of mock data, we verify that unbiased estimates can be obtained for the key cosmological and nuisance parameters, including $S_8$, model parameters of intrinsic alignment, galaxy clustering bias, and shift parameters of the source redshift distributions.
