论文标题
减轻过境调查中的过境时序变化偏差。 ii。河流：开普勒1972年周围的双谐音地球大小的行星从开普勒的误报中恢复
Alleviating the Transit Timing Variations bias in transit surveys. II. RIVERS: Twin resonant Earth-sized planets around Kepler-1972 recovered from Kepler's false positive
论文作者
论文摘要
过境时序变化（TTV）可以通过对观察到的行星的质量和偏心构成约束，甚至限制非交易伴侣的存在，从而为通过Transit观察到的系统提供有用的信息。但是，TTV还可以防止在过境调查中检测小行星，或者偏向回收的行星和过境参数。在这里，我们表明Kepler-1972 C，最初是“不运输的”假阳性KOI-3184.02，是一个地球大小的行星，其轨道受到Kepler-1972 B的扰动（最初是KOI-3184.01）。两人锁定在3：2平均谐振中，每个星球在开普勒任务的持续时间内显示出超过6h小时的TTV。这两个行星具有相似的质量$ m_b/m_c = 0.956 _ { - 0.051}^{+0.056} $和radii $ r_b = 0.802 _ { - 0.041}^{+0.041}^{+0.042} $ r_c = 0.868 _ { - 0.050}^{+0.051} r_ {arter} $，整个系统，包括内部候选KOI-3184.03，似乎是Coplanar。尽管信号的微弱（Kepler-1972 B的每个过境量为1.35，而Kepler-1972 c的SNR为1.35），但我们使用河流方法识别了使用机器学习中河流图中行星轨道的轨道的识别，我们还是使用河流方法恢复了行星的过渡，并恢复了光洁度的河流图和光效应的光洁度拟合。恢复行星的正确晶状体，对于观察到的行星系统的完整图片至关重要。特别是，我们表明，在Kepler-1972中，不考虑行星 - 行星相互作用在行星B和C的半径上产生$ \ sim 30 \％$的误差，除了产生透射式散射外，这会导致错误的koi3184.02的错误。减轻这种偏见对于对开普勒系统，一些苔丝明星和即将到来的柏拉图任务的无偏见至关重要。
Transit Timing Variations (TTVs) can provide useful information for systems observed by transit, by putting constraints on the masses and eccentricities of the observed planets, or even constrain the existence of non-transiting companions. However, TTVs can also prevent the detection of small planets in transit surveys, or bias the recovered planetary and transit parameters. Here we show that Kepler-1972 c, initially the "not transit-like" false positive KOI-3184.02, is an Earth-sized planet whose orbit is perturbed by Kepler-1972 b (initially KOI-3184.01). The pair is locked in a 3:2 Mean-motion resonance, each planet displaying TTVs of more than 6h hours of amplitude over the duration of the Kepler mission. The two planets have similar masses $m_b/m_c =0.956_{-0.051}^{+0.056}$ and radii $R_b=0.802_{-0.041}^{+0.042}R_{Earth}$, $R_c=0.868_{-0.050}^{+0.051}R_{Earth}$, and the whole system, including the inner candidate KOI-3184.03, appear to be coplanar. Despite the faintness of the signals (SNR of 1.35 for each transit of Kepler-1972 b and 1.10 for Kepler-1972 c), we recovered the transits of the planets using the RIVERS method, based on the recognition of the tracks of planets in river diagrams using machine learning, and a photo-dynamic fit of the lightcurve. Recovering the correct ephemerides of the planets is essential to have a complete picture of the observed planetary systems. In particular, we show that in Kepler-1972, not taking into account planet-planet interactions yields an error of $\sim 30\%$ on the radii of planets b and c, in addition to generating in-transit scatter, which leads to mistake KOI3184.02 for a false positive. Alleviating this bias is essential for an unbiased view of Kepler systems, some of the TESS stars, and the upcoming PLATO mission.
