Differential likelihood distribution between the most likely planet-moon model and the other solutions using 10⁶ steps of ourPTMCMC fitting procedure. Left: results from fitting our planet-moon transit model to the original data from Teachey & Kipping (2018). Right: results from fitting our planet-moon transit model to our own detrending of the Kepler and WFC3 data. In both panels the most likely model is located at 0 along the abscissa by definition. In both cases the models do not converge to the best-fit solution, suggesting that the best-fit solution could in fact be an outlier.