TY - JOUR
T1 - A Simplified Photodynamical Model for Planetary Mass Determination in Low-eccentricity Multitransiting Systems
AU - Yoffe, Gideon
AU - Ofir, Aviv
AU - Aharonson, Oded
N1 - We wish to thank Dr. Trifon Trifonov and Yair Judkovsky for helpful discussions, and Prof. Eric Agol for advice on TTVFaster and TTVFast. This study was supported by the Helen Kimmel Center for Planetary Sciences and the Minerva Center for Life Under Extreme Planetary Conditions #13599 at the Weizmann Institute of Science.
PY - 2021/2/10
Y1 - 2021/2/10
N2 - Inferring planetary parameters from transit timing variations (TTVs) is challenging for small exoplanets because their transits may be so weak that determination of individual transit timing is difficult or impossible. We implement a useful combination of tools that together provide a numerically fast global photodynamical model. This is used to fit the TTV-bearing light curve, in order to constrain the masses of transiting exoplanets in low-eccentricity, multiplanet systems-and small planets in particular. We present inferred dynamical masses and orbital eccentricities in four multi-planet systems from Kepler's complete long-cadence data set. We test our model against Kepler-36/KOI-277, a system with some of the most precisely determined planetary masses through TTV inversion methods, and find masses of 5.56(-0.45)(+0.41) and 9.76(-0.89)(+0.79) m(circle plus) for Kepler-36 b and c, respectively-consistent with literature in both value and error. We then improve the mass determination of the four planets in Kepler-79/KOI-152, where literature values were physically problematic to 12.5(-3.6)(+4.5), 9.5(-2.1)(+2.3), 11.3(-2.2)(+2.2) and 6.3(-1.0)(+1.0) m(circle plus) for Kepler-79 b, c, d, and e, respectively. We provide new mass constraints where none existed before for two systems. These are 12.5(-2.6)(+3.2) m(circle plus) for Kepler-450 c, and 3.3(-1.0)(+1.7) and 17.4(-3.8)(+7.1) m(circle plus) for Kepler-595 c (previously KOI-547.03) and b, respectively. The photodynamical code used here, called PyDynamicaLC, is made publicly available.
AB - Inferring planetary parameters from transit timing variations (TTVs) is challenging for small exoplanets because their transits may be so weak that determination of individual transit timing is difficult or impossible. We implement a useful combination of tools that together provide a numerically fast global photodynamical model. This is used to fit the TTV-bearing light curve, in order to constrain the masses of transiting exoplanets in low-eccentricity, multiplanet systems-and small planets in particular. We present inferred dynamical masses and orbital eccentricities in four multi-planet systems from Kepler's complete long-cadence data set. We test our model against Kepler-36/KOI-277, a system with some of the most precisely determined planetary masses through TTV inversion methods, and find masses of 5.56(-0.45)(+0.41) and 9.76(-0.89)(+0.79) m(circle plus) for Kepler-36 b and c, respectively-consistent with literature in both value and error. We then improve the mass determination of the four planets in Kepler-79/KOI-152, where literature values were physically problematic to 12.5(-3.6)(+4.5), 9.5(-2.1)(+2.3), 11.3(-2.2)(+2.2) and 6.3(-1.0)(+1.0) m(circle plus) for Kepler-79 b, c, d, and e, respectively. We provide new mass constraints where none existed before for two systems. These are 12.5(-2.6)(+3.2) m(circle plus) for Kepler-450 c, and 3.3(-1.0)(+1.7) and 17.4(-3.8)(+7.1) m(circle plus) for Kepler-595 c (previously KOI-547.03) and b, respectively. The photodynamical code used here, called PyDynamicaLC, is made publicly available.
UR - http://www.scopus.com/inward/record.url?scp=85101504851&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/abc87a
DO - 10.3847/1538-4357/abc87a
M3 - مقالة
SN - 0004-637X
VL - 908
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 114
ER -