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Removing Imaging Systematics from Galaxy Clustering Measurements with Obiwan: Application to the SDSS-IV extended Baryon Oscillation Spectroscopic Survey Emission Line Galaxy Sample
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2020-09-19 , DOI: 10.1093/mnras/staa2742
Hui Kong 1 , Kaylan J Burleigh 2, 3 , Ashley Ross 1 , John Moustakas 4 , Chia-Hsun Chuang 5 , Johan Comparat 6 , Arnaud de Mattia 7 , Hélion du Mas des Bourboux 8 , Klaus Honscheid 1 , Sichen Lin 9 , Anand Raichoor 7, 10 , Graziano Rossi 11 , Cheng Zhao 7
Affiliation  

This work presents the application of a new tool, Obiwan , which uses image simulations to determine the selection function of a galaxy redshift survey and calculate 3-dimensional (3D) clustering statistics. This is a forward model of the process by which images of the night sky are transformed into a 3D large--scale structure catalog. The photometric pipeline automatically detects and models galaxies and then generates a catalog of such galaxies with detailed information for each one of them, including their location, redshift and so on. Systematic biases in the imaging data are therefore imparted into the catalogs and must be accounted for in any scientific analysis of their information content. Obiwan simulates this process for samples selected from the Legacy Surveys imaging data. This imaging data will be used to select target samples for the next-generation Dark Energy Spectroscopic Instrument (DESI) experiment. Here, we apply Obiwan to a portion of the SDSS-IV extend Baryon Oscillation Spectroscopic Survey Emission Line Galaxies (ELG) sample. Systematic biases in the data are clearly identified and removed. We compare the 3D clustering results to those obtained by the map--based approach applied to the full eBOSS sample. We find the results are consistent, thereby validating the eBOSS ELG catalogs, presented in Raichoor(2020), used to obtain cosmological results.

中文翻译:

使用 Obiwan 从星系团测量中去除成像系统:应用于 SDSS-IV 扩展重子振荡光谱调查发射线星系样本

这项工作介绍了一种新工具 Obiwan 的应用,该工具使用图像模拟来确定星系红移测量的选择函数并计算 3 维 (3D) 聚类统计数据。这是将夜空图像转换为 3D 大型结构目录的过程的正向模型。光度管道会自动检测星系并对其进行建模,然后生成此类星系的目录,其中包含每个星系的详细信息,包括它们的位置、红移等。因此,成像数据中的系统偏差会被赋予目录,并且必须在对其信息内容的任何科学分析中加以考虑。Obiwan 为从 Legacy Surveys 成像数据中选择的样本模拟此过程。该成像数据将用于为下一代暗能量光谱仪 (DESI) 实验选择目标样本。在这里,我们将 Obiwan 应用于 SDSS-IV 扩展重子振荡光谱调查发射线星系 (ELG) 样本的一部分。数据中的系统偏差被清楚地识别和消除。我们将 3D 聚类结果与通过应用于完整 eBOSS 样本的基于地图的方法获得的结果进行比较。我们发现结果是一致的,从而验证了 Raichoor(2020)中提供的用于获得宇宙学结果的 eBOSS ELG 目录。数据中的系统偏差被清楚地识别和消除。我们将 3D 聚类结果与通过应用于完整 eBOSS 样本的基于地图的方法获得的结果进行比较。我们发现结果是一致的,从而验证了 Raichoor(2020)中提供的用于获得宇宙学结果的 eBOSS ELG 目录。数据中的系统偏差被清楚地识别和消除。我们将 3D 聚类结果与通过应用于完整 eBOSS 样本的基于地图的方法获得的结果进行比较。我们发现结果是一致的,从而验证了 Raichoor(2020)中提供的用于获得宇宙学结果的 eBOSS ELG 目录。
更新日期:2020-09-19
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