Figure 1 | The transit light curves for the planets orbiting Kepler-37. The transit model fit to the light curve of Kepler-37 was calculated using a four- parameter nonlinear limb-darkening model that allowed for eccentric orbits. Limb-darkening coefficients were interpolated in stellar temperature, surface gravity and metallicity to determine the appropriate values for Kepler-37, and these were kept fixed. A Markov chain Monte Carlo technique was used to sample the planet parameters to account for correlated variables. The mean stellar density determined by our asteroseismic analysis was used as a prior in the analysis. The three panels show the transits of planets Kepler-37b (a), Kepler-37c (b) and Kepler-37d (c). The photometric light curve has been phase-folded on the orbital period of the planets to show the observed data as a function of orbital phase. Individual data points are shown as black dots. The blue dots show the data binned, with 90, 50 and 30 individual data points making up each binned point in a–c, respectively. The error bar size is the standard deviation of the data making up that bin divided by N1/2, where N is the number of data points in the bin. The best-fitting transit model from the Markov chain Monte Carlo analysis is shown as the red line. The signal-to-noise ratios of the transits of the planets are 13 (a), 49 (b) and 282 (c).