銀河団重力レンズ効果とCMB重力レンズ効果との相関によるニュートリノ質量への制限

我分析开发了一个改进版本的傅立叶幂函数Shapard（FPFS）算法准确和快速的剪切估计。该方法现在包括对困扰所有形状测量算法的偏差源的分析校正：包括噪声偏差（由于可观测量的非线性组合中的噪声）和选择偏差（由于剪切星系或多或少可能被检测到）。至关重要的是，这些分析解决方案不依赖于外部图像模拟的校准。对于孤立星系，小于0.001的乘性偏差和小于0.0001的加性偏差的小残差现在满足第四阶段实验的科学要求。FPFS对暗星系的测量也很准确，对恒星污染也有很强的抵抗能力。一是检验望远镜和大气衍射引起的点扩展函数模型残差在宇宙剪切测量中的系统性。我交叉关联星系的形状与星星的形状，以检测PSF建模残留在星系的形状。另一个零检验是检验弱透镜科学中的B模系统学。然后我研究了重子效应的影响，宇宙剪切测量中的内禀排列的影响。建立了HSC三年弱透镜宇宙学约束的分析流程。

I analytically developed an improved version of the Fourier Power Function Shapelets (FPFS) algorithm for accurate and fast shear estimation. The method now includes analytic corrections for sources of bias that plague all shape measurement algorithms: including noise bias (due to noise in nonlinear combinations of observable quantities) and selection bias (due to sheared galaxies being more or less likely to be detected). Crucially, these analytic solutions do not rely on calibration from external image simulations. For isolated galaxies, the small residual less than 0.001 multiplicative bias and less than 0.0001 additive bias now meet science requirements for Stage IV experiments. FPFS also works accurately for faint galaxies and robustly against stellar contamination.I conducted several systematic null tests for the HSC three-year cosmic shear measurement. One is to test the systematics in cosmic shear measurement caused by model residuals of point spread function due to diffraction of telescope and atmosphere. I cross-correlate galaxy shape with star shape to detect the PSF modelling residual in the galaxy shapes. The other null test is to check the B-mode systematics in the weak-lensing science. Then I looked into the influence of baryonic effect, the influence of the intrinsic alignment in the cosmic shear measurement. I have built up the analysis pipeline for HSC three year weak lensing cosmological constraints.