标题： WFC3/UVIS饱和度图更新 显示英文标题

标题： Updates to the WFC3/UVIS Saturation Map

摘要： 校准软件calwf3用于WFC3/UVIS，使用参考文件来标记超出其全阱深度的饱和像素。 以前，这是通过在整个探测器上使用65,500 e$^{-}$的恒定阈值来完成的。 在本研究中，我们从Mikulski空间望远镜档案（MAST）中检索了$\sim$100万颗恒星，以确定点扩散函数开始变平的通量水平，这发生在中心像素饱和时。 我们在探测器上的1,024个离散区域中量化了饱和极限，并插值得到逐像素的饱和图，以构建现在已集成到calwf3校准管道中的空间可变饱和图参考文件。 我们发现UVIS探测器上的饱和度变化为13%，从63,465 e$^{-}$到72,356 e$^{-}$。 这些值与之前使用稀疏数据集的研究结果一致，当前分析在小尺度上提供了更精确的表征。 关键的是，修订后的饱和值在UVIS探测器的87%以上区域大于之前的恒定阈值，从而在明亮源附近恢复了可用科学像素。 此更新大大提高了使用WFC3/UVIS获得的观测数据质量数组中的饱和标志的鲁棒性，建议用户从MAST重新下载数据以受益于改进的标志。 显示英文摘要

摘要： The calwf3 software for WFC3/UVIS utilizes a reference file to flag pixels that are saturated beyond their full-well depth. Previously, this was accomplished using a constant threshold of 65,500 e$^{-}$ across the entire detector. In this study, we retrieved $\sim$1 million stars from the Mikulski Archive for Space Telescopes (MAST) to determine the flux level at which the Point Spread Function begins to flatten, which occurs as the central pixel saturates. We quantified the saturation limit as a function of position on the detector in 1,024 discrete regions, and interpolated to a pixel-by-pixel saturation map to construct a spatially-variable saturation map reference file that is now implemented in the calwf3 calibration pipeline. We find the saturation varies by 13% across the UVIS detectors, from 63,465 e$^{-}$ to 72,356 e$^{-}$. These values agree well with earlier studies using sparser datasets, with the current analysis leading to improved characterization on small scales. Critically, the revised saturation values are larger than the previous constant threshold over 87% of the UVIS detector, leading to the recovery of usable science pixels near bright sources. This update greatly improves the robustness of saturation flags in the Data Quality arrays of observations obtained with WFC3/UVIS, and users are encouraged to redownload their data from MAST to benefit from the improved flags.