星系 - 半透镜中小尺度的非本地贡献：缓解方案的比较

论文标题

星系 - 半透镜中小尺度的非本地贡献：缓解方案的比较

Non-local contribution from small scales in galaxy-galaxy lensing: Comparison of mitigation schemes

论文作者

Prat, J., Zacharegkas, G., Park, Y., MacCrann, N., Switzer, E. R., Pandey, S., Chang, C., Blazek, J., Miquel, R., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Bernstein, G. M., Chen, R., Choi, A., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Cordero, J., Crocce, M., Davis, C., DeRose, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Krause, E., Kuropatkin, N., Leget, P. -F., McCullough, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sánchez, C., Sanchez, J., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Ferrero, I., Flaugher, B., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Lima, M., Menanteau, F., Mena-Fernández, J., Palmese, A., Paterno, M., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Rodriguez-Monroy, M., Sanchez, E., Schubnell, M., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Weller, J.

论文摘要

最近使用大规模结构和弱透镜测量值（通常称为3 $ \ times $ 2pt）进行的宇宙学分析不得不从小尺度上丢弃大量的信噪比，因为我们无法准确地模拟非线性和Baryonic效应。星系 - 半晶状体镜头或晶状体和源星系之间的位置剪切相关是此类分析中包含的三个两点相关函数之一，通常用平均切向切割剪切估计。但是，在给定角度尺度$θ$或物理规模$ r $的切向剪切测量中，来自以下所有比例的信息，迫使实际数据中应用的比例削减要大于理论上不确定性变得有问题的规模。最近，已经进行了一些独立的努力，旨在减轻星系 - 盖拉克斯镜头信号的非本地性。在这里，我们对不同方法进行比较，包括Y转换，点质量边缘化方法和环形差分表面密度统计。我们在宇宙学的限制水平上进行比较，在联合的星系聚类和星系 - 半透镜分析中进行比较。我们发现，所有估计量都会产生等效的宇宙学结果，假设对空间和时间（LSST）1年的模拟鲁宾天文台遗产调查（如设置）以及应用于DES Y3数据时。使用LSST Y1设置，我们发现缓解方案产生的$ \ sim $ \ sim $ 1.3倍$ S_8 $结果比在不使用任何缓解方案的情况下应用更大的规模削减结果。

Recent cosmological analyses with large-scale structure and weak lensing measurements, usually referred to as 3$\times$2pt, had to discard a lot of signal-to-noise from small scales due to our inability to accurately model non-linearities and baryonic effects. Galaxy-galaxy lensing, or the position-shear correlation between lens and source galaxies, is one of the three two-point correlation functions that are included in such analyses, usually estimated with the mean tangential shear. However, tangential shear measurements at a given angular scale $θ$ or physical scale $R$ carry information from all scales below that, forcing the scale cuts applied in real data to be significantly larger than the scale at which theoretical uncertainties become problematic. Recently there have been a few independent efforts that aim to mitigate the non-locality of the galaxy-galaxy lensing signal. Here we perform a comparison of the different methods, including the Y-transformation, the Point-Mass marginalization methodology and the Annular Differential Surface Density statistic. We do the comparison at the cosmological constraints level in a combined galaxy clustering and galaxy-galaxy lensing analysis. We find that all the estimators yield equivalent cosmological results assuming a simulated Rubin Observatory Legacy Survey of Space and Time (LSST) Year 1 like setup and also when applied to DES Y3 data. With the LSST Y1 setup, we find that the mitigation schemes yield $\sim$1.3 times more constraining $S_8$ results than applying larger scale cuts without using any mitigation scheme.

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