用盖亚周期估计单凌K2行星周期
Estimation of singly-transiting K2 planet periods with Gaia parallaxes
摘要：
当一颗行星只观测到一次凌日时，直接测量其周期是不可能的。然而，限制单次凌日的周期是可能的，这是可取的，因为它们很可能代表任何特定调查所观察到的行星人口的寒冷和极端。因此，提高单次凌日周期约束的准确性对于提高长期行星调查的产量至关重要。在这里，我们结合盖亚星系与恒星模型和宽带测光来估计K2行星宿主恒星的恒星密度，然后使用恒星密度信息来模拟单个行星的凌日并推断后周期分布。我们表明，我们推断的密度是可靠的，通过与通过asteroseismology获得的密度进行比较，并将我们的方法应用于27个已知（直接测量）周期的验证行星，将每次凌日视为唯一的一次，以及12个真正的单凌日。当我们把偏心率作为一个自由参数，我们实现了一个分数周期的不确定性超过真正的单次过境的$94^{+87}_{-58}\%$，当我们固定$e=0$，我们实现分数周期的不确定性$15^{+30}_{-6}\%$，一个大约三倍的改进，典型的周期不确定性的以前的研究。
英文摘要：
When a planet is only observed to transit once, direct measurement of its period is impossible. It is possible, however, to constrain the periods of single transiters, and this is desirable as they are likely to represent the cold and far extremes of the planet population observed by any particular survey. Improving the accuracy with which the period of single transiters can be constrained is therefore critical to enhance the long-period planet yield of surveys. Here, we combine Gaia parallaxes with stellar models and broad-band photometry to estimate the stellar densities of K2 planet host stars, then use that stellar density information to model individual planet transits and infer the posterior period distribution. We show that the densities we infer are reliable by comparing with densities derived through asteroseismology, and apply our method to 27 validation planets of known (directly measured) period, treating each transit as if it were the only one, as well as to 12 true single transiters. When we treat eccentricity as a free parameter, we achieve a fractional period uncertainty over the true single transits of $94^{+87}_{-58}\%$, and when we fix $e=0$, we achieve fractional period uncertainty $15^{+30}_{-6}\%$, a roughly threefold improvement over typical period uncertainties of previous studies.
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