eROSITA X射线源探测策略的建立与仿真
Establishing the X-ray Source Detection Strategy for eROSITA with Simulations
摘要：
光谱-伦琴-伽马（SRG）卫星上的eROSITA X射线望远镜已开始以前所未有的速度在全天空探测新的X射线源。了解源探测的性能和选择功能对于后续eROSITA星表的科学分析非常重要。通过模拟，我们测试和优化eROSITA源检测程序，我们定量表征检测目录。以eROSITA最终赤道深度调查（eFEDS）为例，我们根据我们对仪器特性、背景光谱和天文X射线源数量的最佳了解，进行了广泛的光子事件模拟。我们介绍了一种分析源检测的完整性，纯度和效率的基础上每个光子的起源的方法。根据模拟中测得的源探测效率，我们选择了一种双管齐下的策略来构建eROSITA X射线目录，创建一个主目录，只使用最敏感的波段（0.2 - 2.3 keV）和一个独立的硬带选择目录，使用多波段探测范围高达5 keV。由于我们的模拟数据高度代表真实的eFEDS数据，我们使用模拟目录来测量eFEDS目录的完整性和纯度作为多个参数的函数，例如检测可能性，通量和光度。这些测量为选择eFDS目录选择阈值提供了基础。模拟星表（本文提供）可用于构造活动星系核和星系团的选择函数。输出和输入模拟目录的直接比较也产生了一个校正曲线，将原始点源通量分布转换为内禀数计数分布。
英文摘要：
The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures, and we characterize the detected catalog quantitatively. Taking the eROSITA Final Equatorial-Depth Survey (eFEDS) as an example, we ran extensive photon-event simulations based on our best knowledge of the instrument characteristics, the background spectrum, and the population of astronomical X-ray sources. We introduce a method of analyzing source detection completeness, purity, and efficiency based on the origin of each photon. According to the source detection efficiency measured in the simulation, we chose a two-pronged strategy to build eROSITA X-ray catalogs, creating a main catalog using only the most sensitive band (0.2-2.3 keV) and an independent hard-band-selected catalog using multiband detection in a range up to 5 keV. Because our mock data are highly representative of the real eFEDS data, we used the mock catalogs to measure the completeness and purity of the eFEDS catalogs as a function of multiple parameters, such as detection likelihood, flux, and luminosity. These measurements provide a basis for choosing the eFEDS catalog selection thresholds. The mock catalogs (available with this paper) can be used to construct the selection function of active galactic nuclei and galaxy clusters. A direct comparison of the output and input mock catalogs also gives rise to a correction curve that converts the raw point-source flux distribution into the intrinsic number counts distribution.
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