Fig. 3: Transit light curves of Kepler-1708 b.
From: Large exomoons unlikely around Kepler-1625 b and Kepler-1708 b
The out-of-Hill-sphere parts of the Kepler-1708 b transit light curves were detrended using a biweight filter and the LDCs were used as free fitting parameters. a,b, Blue and orange lines visualize 67 planet-only models and 33 planet–moon models, respectively, that were randomly drawn from the respective posterior distributions for transit 1 (a) and transit 2 (b). The number of light curves represents the corresponding Bayes factor Bmp = 0.5, which means that the planet-only interpretation is twice as probable as the planet–moon interpretation. The best-fitting models of a planet only and of a planet with a moon are shown with dashed and solid black lines, respectively. c,d, Residuals of the observed data and the best fit of the planet-only model for transit 1 (c) and transit 2 (d). Red lines denote the five-bin walking mean. e,f, Residuals of the observed data and the best fit of the planet–moon model for transit 1 (e) and transit 2 (f). ppt, parts per thousand.
