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Of the over 450 exoplanets known to date, more than 420 of them have beendiscovered using radial velocity studies, a method that tells nothing about theinclination of the planet's orbit. Because it is more likely that the companionis a planetary-mass object in a moderate- to high-inclination orbit than alow-mass stellar object in a nearly face-on orbit, the secondary bodies arepresumed to be planets. Interferometric observations allow us to inspect theangular diameter fit residuals to calibrated visibilities in order to rule outthe possibility of a low-mass stellar companion in a very low-inclinationorbit. We used the Center for High Angular Resolution Astronomy (CHARA) Arrayinterferometer to observe 20 exoplanet host stars and considered five potentialsecondary spectral types: G5 V, K0 V, K5 V, M0 V, and M5 V. If a secondary staris present and is sufficiently bright, the effects of the added light willappear in interferometric observations where the planet will not. All secondarytypes could be eliminated from consideration for 7 host stars and no secondarystars of any spectral type could be ruled out for 7 more. The remaining 6 hoststars showed a range of possible secondary types.

Ruling Out Possible Secondary Stars to Exoplanet Host Stars Using the CHARA Array