The Kepler Eclipsing System KIC 5621294 and its Substellar Companion

Abstract

We present the physical properties of KIC 5621294 showing light and timing variations from the $Kepler$ photometry. Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76${}^{\circ }$.8, and $\Delta$($T_1$--$T_2$)=4,235 K, in which the detached primary component fills about 77\% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \& van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3\sin i_3$=46.9 M${}_{\mathrm{Jup}}$, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40${}^{\circ }$, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or an angular momentum via magnetic braking. It is possible that the parabola may only be the observed part of a period modulation caused by the presence of another companion in a wider orbit.

arXiv comment19 pages, including 5 figures and 4 tables, accepted for publication in AJ

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