Single transit survey in CoRoT, Kepler, K2 and TESS light curves

今天已知的大多数已确认的行星都是在太空任务CoRoT、开普勒、K2和TESS的高分辨率恒星光曲线中发现的。这些光曲线由于数据量大，需要通过自动检测管道寻找候选光曲线。大多数检测方法使用盒租方（BLS）算法或频率分析（例如FFT，小波分析）利用光曲线中过境的周期性。这些算法通常需要至少三次凌日来验证检测（光曲线超过凌日轨道周期长度的两倍）。在光曲线中只有一次可见的行星（单次凌日，单次凌日）通常不会被这些自动管道检测到。双星或大行星（木星行星）的单次凌日是通过目视搜索或通过分析多行星系统的探测发现的。大多数浅层行星单次凌日（海王星、超级地球行星）仍然隐藏在存档数据中。特别是K2和TESS的相对较短的光曲线必须包含许多周期长达100天的行星单次凌日。建议在现有的CoRoT、Kepler、K2和TESS的存档数据中搜索未知的单次凌日，特别是小行星。现有的基于小波的瞬态搜索算法（SINGLETRANS）应发展成全自动管道。对新增的候选卫星进行分析，估计轨道参数。新发现的候选行星应添加到候选行星列表中，以填充轨道周期较大的候选行星区域。SINGLETRANS管道也适用于探测周期和“准周期”（强TTV，环双行星）凌日。对检测到的候选集合进行广泛的统计分析，并将SINGLETRANS的结果与广泛使用的BLS算法进行比较。应选择合适的候选人在KESPRINT合作中进行跟踪。额外发现的轨道周期较大的候选行星数量将有助于了解系外行星的多样性。

Most confirmed planets known today were detected in high resolution stellar light curves of the space missions CoRoT, Kepler, K2 and TESS. These light curves are searched for candidates by automatic detection pipelines because of the large data amount. Most detection methods make use of the periodicity of the transits in the light curve using box leased square (BLS) algorithm or frequency analysis (e.g. FFT, wavelet analysis). These algorithms usually need three transits at least for a verified detection (light curves more than two times the length of the orbital period of the transit). Planets with only one transit visible in the light curve (single transits, mono transits) are usually not detected with these automatic pipelines. Single transits of binaries or large planets (Jupiter planets) were found by visual search or by analysis of detections in multi-planet systems. Most of the planetary single transits of shallow depth (Neptune, Super-Earth planets) are still hidden in the archived data. In particular the relatively short light curves of K2 and TESS must include many single transits of planets up to a period of 100 days. It is proposed to search the available archived data of CoRoT, Kepler, K2 and TESS for unknown single transits of especially small planets. An existing transient search algorithm based on wavelets (SINGLETRANS) shall be developed into a fully automatic pipeline. The additional new candidates shall be analyzed and the orbital parameters shall be estimated. New detected candidates shall be added to the candidate list to populate the area of planetary candidates with larger orbital periods. The SINGLETRANS pipeline shall be suitable to detect also periodic and ‘quasi periodic’ (strong TTV, circum-binary planets) transits. An extensive statistical analysis of the detected candidate ensemble and a comparison between the results of SINGLETRANS and the widely used BLS algorithm shall be performed. Suitable candidates shall be selected for follow-up inside the KESPRINT collaboration. The additional number of detected candidates with larger orbital periods shall help to understand the diversity of exoplanets.