Dark Energy Survey year 3 results: point spread function modelling
Dark Energy Survey year 3 results: point spread function modelling
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DOI：
10.1093/mnras/staa3679
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发表时间：
2020-11
影响因子：
4.8
通讯作者：
M. Jarvis;G. Bernstein;A. Amon;C. Davis;P. L'eget;K. Bechtol;I. Harrison;M. Gatti;A. Roodman
中科院分区：
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作者：
M. Jarvis;G. Bernstein;A. Amon;C. Davis;P. L'eget;K. Bechtol;I. Harrison;M. Gatti;A. Roodman
我们介绍了一个新的软件包，用于模拟点扩散函数（PSF）的天文图像，称为piff（PSF在全视场），我们适用于前三年（称为Y3）的暗能量调查（DES）数据。我们描述了piff用于模拟PSF的算法的相关细节，包括PSF模型如何在视场（FOV）中变化。诊断结果表明，从PSF建模的系统误差是非常小的范围内的规模是很重要的DES Y3弱透镜分析。特别是，PSF建模的系统误差明显小于DES第一年（Y1）分析的相应结果。我们还简要介绍了一些计划的改进，我们希望在未来的分析，以进一步减少建模误差。
We introduce a new software package for modelling the point spread function (PSF) of astronomical images, called piff (PSFs In the Full FOV), which we apply to the first three years (known as Y3) of the Dark Energy Survey (DES) data. We describe the relevant details about the algorithms used by piff to model the PSF, including how the PSF model varies across the field of view (FOV). Diagnostic results show that the systematic errors from the PSF modelling are very small over the range of scales that are important for the DES Y3 weak lensing analysis. In particular, the systematic errors from the PSF modelling are significantly smaller than the corresponding results from the DES year one (Y1) analysis. We also briefly describe some planned improvements to piff that we expect to further reduce the modelling errors in future analyses.