Kepler eclipse timings of KIC 9472174

The light curve shows both primary and secondary eclipses, along with a strong reflection effect from the cool companion. Here, we present constraints on the component masses and eccentricity derived from the Romer delay of the secondary eclipse.

Using six months of publicly available Kepler photometry obtained in short-cadence mode, we fit model profiles to the primary and secondary eclipses to measure their centroid values. We find that the secondary eclipse arrives on average 2.06+/-0.12s after the midpoint between primary eclipses. Under the assumption of a circular orbit, we calculate from this time delay a mass ratio of q=0.2691+/-0.0018 and individual masses of M_sd_=0.372+/-0.024M_{sun}_ and M_c_=0.1002+/-0.0065M_{sun}_ for the sdB and M dwarf, respectively.