论文标题
搜索围绕热分子的二线ii周围的过境行星。补充方法和苔丝周期1的结果
A search for transiting planets around hot subdwarfs II. Supplementary methods and results from TESS Cycle 1
论文作者
论文摘要
语境。热式和小的燃烧物体是热的细胞绘制物，是探索红色巨型分支（RGB）后行星系统演变的理想目标。到目前为止，尚未确认它们的行星，并且还没有进行系统的调查来查找行星。目标。在这个项目中，我们旨在通过来自太空望远镜（Kepler，K2，Tess和Cheops）的所有光线曲线进行系统的过境调查。目的是在两个点上计算有意义的统计数据：首先，围绕热分子的行星的发生率，其次，在其宿主的RGB阶段吞没的近距离行星生存的可能性。本文重点介绍了苔丝任务1周期中进行的观察结果的分析。方法。我们使用了专门设计的管道夏洛克（Sherlock）在可用的光曲线中搜索过境。当检测到信号时，在对象有资格进行后续观察和深入分析以确定过境体的性质之前，将在下一个评估阶段进行处理。结果。我们将方法应用于苔丝周期1期间观察到的792个热分子。尽管在光曲线中检测到378个有趣的信号，但只有26颗恒星被分配以进行后续观察。我们已经确定了一系列黯然失色的二进制文件，过境的白矮人和其他类型的假阳性，但迄今为止尚未确认行星。第一次计算出现率的上限是用显示未信号的549个目标进行的。结论。我们开发的工具和方法证明了它们在分析太空任务的可用光曲线方面的效率，从检测有趣的信号到识别过境星球。这将使我们能够实现该项目的两个主要目标。
Context. Hot subdwarfs, which are hot and small He-burning objects, are ideal targets for exploring the evolution of planetary systems after the red giant branch (RGB). Thus far, no planets have been confirmed around them, and no systematic survey to find planets has been carried out. Aims. In this project, we aim to perform a systematic transit survey in all light curves of hot subdwarfs from space-based telescopes (Kepler, K2, TESS, and CHEOPS). The goal is to compute meaningful statistics on two points: firstly, the occurrence rates of planets around hot subdwarfs, and secondly, the probability of survival for close-in planets engulfed during the RGB phase of their host. This paper focuses on the analysis of the observations carried out during cycle 1 of the TESS mission. Methods. We used our specifically designed pipeline SHERLOCK to search for transits in the available light curves. When a signal is detected, it is processed in the next evaluating stages before an object is qualified for follow-up observations and in-depth analysis to determine the nature of the transiting body. Results. We applied our method to the 792 hot subdwarfs observed during cycle 1 of TESS. While 378 interesting signals were detected in the light curves, only 26 stars were assigned for follow-up observations. We have identified a series of eclipsing binaries, transiting white dwarfs, and other types of false positives, but no planet has been confirmed thus far. A first computation of the upper limit for occurrence rates was made with the 549 targets displaying no signal. Conclusions. The tools and method we developed proved their efficiency in analysing the available light curves from space missions, from detecting an interesting signal to identifying a transiting planet. This will allow us to fulfil the two main goals of this project.
