论文标题
珀金斯红外外卫星调查（PINES）II。过境候选者及其对L和T矮人周围行星的影响
The Perkins INfrared Exosatellite Survey (PINES) II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
论文作者
论文摘要
我们描述了一种新的过境检测算法，该算法旨在检测不连续的Perkins红外外卫星调查（PINES）观察到L和T矮人的观察结果。我们使用该算法在131个PINES光曲线中搜索过境，并识别两个过境候选者：2MASS J18212815+1414010（2MASS J1821+1414）和2MASS J08350622+1953050（2MASS J0835+1953）。由于源的已知可变性属性，我们不喜欢2MASS J1821+1414作为真正的过境候选者。我们不能排除2MASS J0835+1953的候选事件的行星性质，并执行后续观察，以试图恢复第二次过境。重复事件尚未观察到，但是这些观察结果表明，目标变异性是候选运输的不可能的原因。我们对光曲线进行了马尔可夫链蒙特卡洛模拟，并估计行星半径范围从$ 4.2^{+3.5} _ { - 1.6} r_ \ oplus $到$ 5.8^{+4.8} _ {+4.8} _ { - 2.1} r_ \ oplus $，取决于主机的年龄。最后，我们对光曲线样品进行注射和恢复模拟。我们使用测得的M矮星行星的发生率将行星注入数据中，并尝试使用我们的Transit搜索算法将它们恢复。我们的检测率表明，假设行星的发生率，我们应该大约有1 $ \％$的机会来检测可能导致我们观察到的2MASS J0835+1953的候选者。如果确认了2MASS J0835+1953 B，则与M矮人相比，L和T矮人周围的短周期行星的发生有所提高，这将挑战行星形成模型的预测。
We describe a new transit detection algorithm designed to detect single transit events in discontinuous Perkins INfrared Exosatellite Survey (PINES) observations of L and T dwarfs. We use this algorithm to search for transits in 131 PINES light curves and identify two transit candidates: 2MASS J18212815+1414010 (2MASS J1821+1414) and 2MASS J08350622+1953050 (2MASS J0835+1953). We disfavor 2MASS J1821+1414 as a genuine transit candidate due to the known variability properties of the source. We cannot rule out the planetary nature of 2MASS J0835+1953's candidate event and perform follow-up observations in an attempt to recover a second transit. A repeat event has yet to be observed, but these observations suggest that target variability is an unlikely cause of the candidate transit. We perform a Markov chain Monte Carlo simulation of the light curve and estimate a planet radius ranging from $4.2^{+3.5}_{-1.6}R_\oplus$ to $5.8^{+4.8}_{-2.1}R_\oplus$, depending on the host's age. Finally, we perform an injection and recovery simulation on our light curve sample. We inject planets into our data using measured M dwarf planet occurrence rates and attempt to recover them using our transit search algorithm. Our detection rates suggest that, assuming M dwarf planet occurrence rates, we should have roughly a 1$\%$ chance of detecting a candidate that could cause the transit depth we observe for 2MASS J0835+1953. If 2MASS J0835+1953 b is confirmed, it would suggest an enhancement in the occurrence of short-period planets around L and T dwarfs in comparison to M dwarfs, which would challenge predictions from planet formation models.
