SDSS-V DR20观测到的SRG/eROSITA X射线选激变变星候选体
SRG/eROSITA X-ray selected cataclysmic variable candidates observed in SDSS-V DR20
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中文总结 AI 辅助
本研究结合eROSITA X射线数据与SDSS-V、Gaia光学数据，通过三种方法识别激变变星候选体，共确认587个激变变星，助力理解银河系激变变星的演化与分布。
中文摘要 AI 辅助
我们报告了SDSS-V DR20期间对吸积致密双星（ACB）的光谱观测，具体为激变变星（CVs），这些天体是从SRG（Spectrum Roentgen Gamma）eROSITA的eRASS1和eRASS:3观测中被识别为可能的致密双星候选体。我们的主要目标是获得在eRASS1和eRASS:3中探测到的所有CVs的完整列表，以帮助更好地理解密近双星演化、这些系统在银河系中的空间密度和人口统计学特征。之前的人口研究各有局限性：体积受限样本存在统计数量不足的问题，而星等受限观测则偏向于仅更明亮的系统。所有CVs都是X射线辐射体，因此eROSITA提供了一个基于X射线辐射识别CVs的独特机会。考虑到eROSITA的灵敏度，我们预计会在500秒差距内发现大多数X射线活跃的CVs，而磁CVs则可在数千秒差距内被发现。结合eROSITA的X射线数据和Gaia的光学数据，我们探索了三种不同的方法来识别eROSITA X射线源的Gaia光学对应体，这些源属于可能的ACB。由此，我们识别出独特的候选体，并将其作为三个不同的观测方案提交给SDSS-V，作为银河系测绘者（Milky Way Mapper）巡天的一部分进行光学光谱观测。从我们提交的候选体中，我们发现了538个可能的CVs。我们还在其他基于eROSITA的观测方案中识别出了CVs，其中又发现了49个可能的CVs系统，这些系统不在我们的初选范围内。因此，通过基于eROSITA的SDSS-V观测，我们共识别出587个CVs系统。我们还尝试基于eROSITA的X射线数据、SDSS-V光学光谱中的发射线特性以及公开领域的其他可用数据，将这些CVs细分为矮新星、类新星或磁系统。
英文摘要
We report on the spectroscopic observations obtained during SDSS-V DR20 of accreting compact binaries (ACB), specifically the cataclysmic variables (CVs), that were identified as likely compact binary candidates from the SRG (Spectrum Roentgen Gamma) eROSITA eRASS1 and eRASS:3 observations. Our primary aim is to obtain a complete inventory of all CVs that were detected in eRASS1 and eRASS:3, with the goal to help better understand close-binary evolution, the population density, and demographics of these systems in the Galaxy. Previous population studies had their respective limitations, with volume-limited samples suffering from low-number statistics, while magnitude-limited observations were biased to only the brighter systems. All CVs are X-ray emitters, eROSITA, therefore, presents a unique opportunity to identify CVs based on their X-ray emission. Given eROSITA's sensitivity, we expect to find most X-ray active CVs within 500 pc, and magnetic CVs to several kpc. Using X-ray data from the eROSITA together with optical data from Gaia, three different approaches were explored to identify the Gaia optical counterpart to the eROSITA X-ray source of the likely ACB. From this, unique candidates were identified and were submitted in three different cartons to SDSS-V for optical spectroscopic observations as part of the Milky Way Mapper survey. From our submitted candidates, we found 538 likely CVs. We also identified CVs that were observed in other eROSITA based cartons, in which we identified an additional 49 systems that are likely CVs and which were not in our selection. We therefore identified 587 systems as CVs from the eROSITA based SDSS-V observations. We also attempted to sub classify the CVs as dwarf-novae, novalikes, or magnetic systems based on the eROSITA X-ray data, the emission line properties in the optical SDSS-V spectra, and other data in the public domain, if available.
