Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Author(s): Wang, S; Wu, DH; Addison, BC; Laughlin, G; Liu, HG; Wang, YH; Yang, T; Yang, M; Yisikandeer, A; Hong, R; Li, B; Liu, J; Zhao, H; Wu, ZY; Hu, SM; Zhou, X; Zhou, JL; Zhang, H; Zheng, J; Wang, W; Fan, Z; Niu, H; Chen, YY; Lu, H; Peng, X; Li, K; Guo, DF | Abstract: © 2018. The American Astronomical Society. All rights reserved. The Kepler-9 system harbors three known transiting planets. The system holds significant interest for several reasons. First, the outer two planets exhibit a period ratio that is close to a 2:1 orbital commensurability, with attendant dynamical consequences. Second, both planets lie in the planetary mass "desert" that is generally associated with the rapid gas agglomeration phase of the core accretion process. Third, there exist attractive prospects for accurately measuring both the sky-projected stellar spin-orbit angles as well as the mutual orbital inclination between the planets in the system. Following the original Kepler detection announcement in 2010, the initially reported orbital ephemerides for Kepler-9 b and c have degraded significantly, due to the limited time base-line of observations on which the discovery of the system rested. Here, we report new ground-based photometric observations and extensive dynamical modeling of the system. These efforts allow us to photometrically recover the transit of Kepler-9 b and thereby greatly improve the predictions for upcoming transit mid-times. Accurate ephemerides of this system are important in order to confidently schedule follow-up observations of this system, for both in-transit Doppler measurements as well as for atmospheric transmission spectra taken during transit.