论文标题
绕着M星的行星的发生率：将ABC应用于开普勒DR25，Gaia DR2和2MASS数据
Occurrence Rates of Planets Orbiting M Stars: Applying ABC to Kepler DR25, Gaia DR2, and 2MASS Data
论文作者
论文摘要
我们介绍了在M颗星附近的Kepler行星候选候选的强劲行星发生率，用于行星Radii $ r_p = 0.5-4〜 \ textrm {r} _ \ oplus $和Orbital时期$ p = 0.5-256 $ p = 0.5-256 $ days使用大约贝叶斯计算（ABC）技术。这项工作结合了最终的开普勒DR25行星候选目录和数据产品，并使用Gaia DR2和2 Mass PSC增强了它们的更新恒星属性。我们应用一组选择标准，以选择1,746个开普勒M矮人目标的样本，该目标容纳89个相关的行星候选。这些早期的M矮人和晚期K矮人是使用Gaia DR2的几个光度质量标志和使用2个质量幅度的颜色降低的近距参考目标中选择的。我们估计一个可居住区的出现率为$ f _ {\ textrm {m，hz}} = 0.33^{+0.10} _ { - 0.12} $，用于行星，$ 0.75-1.5 $ r $ $ _ \ oplus $ size。我们警告说，由于目标恒星和行星候选物的样本较小，开普勒M恒星的发生率估计值对先验的选择敏感。例如，我们发现出现$ 4.2^{+0.6} _ { - 0.6} $或$ 8.4^{+1.2} _ { - 1.1} $ Planets $ Planets $ Planets $ Planets $ Planets $ dwarf（在$ r_p = 0.5-4〜 \ textrm {r} _ \ r} _ \ oplus $和$ p $ p = 0.56的$ r_p = 0.5-4〜 \ textrm {r}在相同的轨道周期比较时，这些发生率大于FGK矮人目标的发生率，但在计算作为同等恒星失去的函数时类似于发生率。将我们的结果与最近对系外行星架构的研究相结合，表明大多数，也可能是早期的M矮人港口行星系统。
We present robust planet occurrence rates for Kepler planet candidates around M stars for planet radii $R_p = 0.5-4~\textrm{R}_\oplus$ and orbital periods $P = 0.5-256$ days using the approximate Bayesian computation (ABC) technique. This work incorporates the final Kepler DR25 planet candidate catalog and data products and augments them with updated stellar properties using Gaia DR2 and 2MASS PSC. We apply a set of selection criteria to select a sample of 1,746 Kepler M dwarf targets that host 89 associated planet candidates. These early M dwarfs and late K dwarfs were selected from cross-referenced targets using several photometric quality flags from Gaia DR2 and color-magnitude cuts using 2MASS magnitudes. We estimate a habitable zone occurrence rate of $f_{\textrm{M,HZ}} = 0.33^{+0.10}_{-0.12}$ for planets with $0.75-1.5$ R$_\oplus$ size. We caution that occurrence rate estimates for Kepler M stars are sensitive to the choice of prior due to the small sample of target stars and planet candidates. For example, we find an occurrence rate of $4.2^{+0.6}_{-0.6}$ or $8.4^{+1.2}_{-1.1}$ planets per M dwarf (integrating over $R_p = 0.5-4~\textrm{R}_\oplus$ and $P = 0.5-256$ days) for our two choices of prior. These occurrence rates are greater than those for FGK dwarf target when compared at the same range of orbital periods, but similar to occurrence rates when computed as a function of equivalent stellar insolation. Combining our result with recent studies of exoplanet architectures indicates that most, and potentially all, early-M dwarfs harbor planetary systems.
