VizieR Online Data Catalog: Transits of PH3 b, c, and d through January, 2019 (Schmitt+, 2014)

Using quarters 1-16 of the Kepler data, we extracted and flattened each transit using the IDL AutoKep program (Gazak et al. 2012AdAst2012E..30G). For the high signal-to-noise transits of the outer planet, we used short cadence data where available. We then used a new, modified version of the IDL program TAP (Carter & Winn, 2009ApJ...704...51C; Gazak et al. 2012AdAst2012E..30G; Eastman et al. 2013PASP..125...83E) to fit for the orbital parameters of each planet: impact parameter (b), duration (T), the ratio of planet radius to stellar radius (R_p/R_*), the midtransit times, linear limb darkening, quadratic limb darkening (Kipping, 2013MNRAS.435.2152K), and white and red noise. The ratio of semi-major axis to the radius of the star (a/R_*) and the inclination (i) can be derived from these parameters.

(1 data file).