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KOI-13.01, a planet-sized companion in an optical double star was announcedas one of the 1235 Kepler planet candidates in February 2011. The transitcurves show significant distortion that was stable over the ~130 days time-spanof the data. Here we investigate the phenomenon via detailed analyses of thetwo components of the double star and a re-reduction of the Kepler data withpixel-level photometry. Our results indicate that KOI-13 is a common propermotion binary, with two rapidly rotating components (v sin i ~ 65--70 km/s). Weidentify the host star of KOI-13.01 and conclude that the transit curveasymmetry is consistent with a companion orbiting a rapidly rotating, possiblyelongated star on an oblique orbit. After correcting the Kepler light curve tothe second light of the optical companion star, we derive a radius of 2.2 R_Jfor the transiter, implying an irradiated late-type dwarf, probably a hot browndwarf rather than a planet. KOI-13 is the first example for detecting orbitalobliquity for a substellar companion without measuring the Rossiter-McLaughlineffect from spectroscopy.

Asymmetric transit curves as indication of orbital obliquity: clues from the late-type dwarf companion in KOI-13