http://arxiv.org/abs/1909.02427
We present the discovery of Kepler-88 d ($P_d = 1414^{+27}{-23}$ days, $M$sin$i_d = 959\pm57\,M\oplus$, $e_d = 0.432\pm0.048$) based on six years of radial velocity (RV) follow-up from the W. M. Keck Observatory HIRES spectrograph. Kepler-88 has two previously identified planets: Kepler-88 b (KOI-142.01) transits in the NASA Kepler photometry and has very large transit timing variations. Nesvorny et al. (2013) perfomed a dynamical analysis of the TTVs to uniquely identify the orbital period and mass of the perturbing planet (Kepler-88 c), which was later was confirmed with RVs from the Observatoire Haute-Provence (OHP, Barros2014). To fully explore the architecture of this system, we performed photodynamical modeling on the Kepler photometry combined with the RVs from Keck and OHP and stellar parameters from spectroscopy and Gaia. Planet d is not detectable in the photometry, and long-baseline RVs are needed to ascertain its presence. However, the orbital parameters and masses of interacting planets b and c are improved by an order of magnitude with respect to the RV-only solution when the photometry is included: $P_b =10.91647\pm0.00014$ days, $M_b=9.5\pm 1.2\,M_\oplus$, $P_c=22.2649\pm0.0007$ days, and $M_c=214.2\pm5.2\,M_\oplus$. The photodynamical solution also finds that planets b and c have low eccentricites, are apsidally anti-aligned, and have conjunctions on the same hemisphere of the star. Continued RV follow-up of systems with small planets will improve our understanding of the link between inner planetary system architectures and giant planets.
L. Weiss, E. Agol, D. Fabrycky, et. al.
Fri, 6 Sep 19
74/78
Comments: 24 pages, submitted to AJ