完备性校正方法的定量评估和通用模拟代码的公开发布
A quantitative assessment of completeness correction methods and public release of a versatile simulation code
摘要：
具有准确的完整性函数是至关重要的，以确定的休息帧紫外光度函数（UVLF）的所有方式回到时代的再电离。大多数研究使用注入采收率模拟来确定完备性函数。虽然概念上相似，但已发表的方法在完整性函数的定义上有细微但重要的差异。因此，他们采用不同的方法来确定UVLF。我们讨论了现有方法的优点和局限性，使用一组模拟观测，然后比较的方法时，适用于同一组哈勃遗产领域（HLF）的图像。我们发现，在我们所有的模拟观测下，最稳健的方法是将完整性定义为输入和输出幅度的函数的方法。仅将完整性考虑为输入或输出幅度的函数的其他方法可能在存在光度散射和/或陡峭光度函数的情况下受到限制。特别是，当通量散射>0.2 mag时，UVLF亮端的偏差与其他系统效应（如透镜放大率偏差）相当。在HLF图像上进行测试时，所有方法产生的UVLF在2 sigma置信度内是一致的，这表明文献中的UVLF不确定性仍然由小数统计和宇宙方差主导。本研究中使用的完整性模拟代码（GLACiaR 2）与本文一起公开发布，作为分析未来更高精度数据集的工具，例如詹姆斯韦伯太空望远镜的预期数据集。
英文摘要：
Having accurate completeness functions is crucial to the determination of the rest-frame ultraviolet luminosity functions (UVLFs) all the way back to the epoch of reionization. Most studies use injection-recovery simulations to determine completeness functions. Although conceptually similar, published approaches have subtle but important differences in their definition of the completeness function. As a result, they implement different methods to determine the UVLFs. We discuss the advantages and limitations of existing methods using a set of mock observations, and then compare the methods when applied to the same set of Hubble Legacy Field (HLF) images. We find that the most robust method under all our mock observations is the one that defines completeness as a function of both input and output magnitude. Other methods considering completeness only as a function of either input or output magnitude may suffer limitations in a presence of photometric scatter and/or steep luminosity functions. In particular, when the flux scatter is >0.2 mag, the bias in the bright end of the UVLFs is on par with other systematic effects such as the lensing magnification bias. When tested on HLF images, all methods yield UVLFs that are consistent within 2 sigma confidence, suggesting that UVLF uncertainties in the literature are still dominated by small number statistics and cosmic variance. The completeness simulation code used in this study (GLACiaR2) is publicly released with this paper as a tool to analyze future higher precision datasets such as those expected from the James Webb Space Telescope.
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