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We present an algorithm to search for the faint spectrum of a second starmixed with the spectrum of a brighter star in high resolution spectra. We modeloptical stellar spectra as the sum of two input spectra drawn from a vastlibrary of stars throughout the H-R diagram. From typical spectra havingresolution of R=60,000, we are able to detect companions as faint as 1%relative to the primary star in approximately the V and R bandpasses ofphotometry. We are also able to find evidence for triple and quadruple systems,given that any additional companions are sufficiently bright. The precisethreshold percentage depends on the SNR of the spectrum and the properties ofthe two stars. For cases of non-detection, we place a limit on the brightnessof any potential companions. This algorithm is useful for detecting both faintorbiting companions and background stars that are angularly close to aforeground target star. The size of the entrance slit to the spectrometer, 0.87x 3 arcsec (typically), sets the angular domain within which the second starcan be detected. We analyzed Keck-HIRES spectra of 1160 California KeplerSurvey objects of interest (KOI) searching for the secondary spectra, with thetwo goals of alerting the community to two possible host stars of thetransiting planet and to dilution of the light curve. We report 63 CaliforniaKepler Survey objects of interest showing spectroscopic evidence of a secondarystar.

Detection of Stars within $\sim$0.8 arcseconds of Kepler Objects of Interest