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(Abbreviated) Kepler planet candidates require both spectroscopic and imagingfollow-up observations to rule out false positives and detect blended stars.[...] In this paper, we examine a sample of 11 Kepler host stars withcompanions detected by two techniques -- near-infrared adaptive optics and/oroptical speckle interferometry imaging, and a new spectroscopic deblendingmethod. We compare the companion Teff and flux ratios (F_B/F_A, where A is theprimary and B is the companion) derived from each technique, and find no caseswhere both companion parameters agree within 1sigma errors. In 3/11 cases thecompanion Teff values agree within 1sigma errors, and in 2/11 cases thecompanion F_B/F_A values agree within 1sigma errors. Examining each Keplersystem individually considering multiple avenues (isochrone mapping, contrastcurves, probability of being bound), we suggest two cases for which thetechniques most likely agree in their companion detections (detect the samecompanion star). Overall, our results support the advantage the spectroscopicdeblending technique has for finding very close-in companions ($\theta\lesssim$0.02-0.05") that are not easily detectable with imaging. However, wealso specifically show how high-contrast AO and speckle imaging observationsdetect companions at larger separations ($\theta \geq$0.02-0.05") that aremissed by the spectroscopic technique, provide additional information forcharacterizing the companion and its potential contamination (e.g., PA,separation, $\Delta$m), and cover a wider range of primary star effectivetemperatures. The investigation presented here illustrates the utility ofcombining the two techniques to reveal higher-order multiples in knownplanet-hosting systems.

A Comparison of Spectroscopic versus Imaging Techniques for Detecting Close Companions to Kepler Objects of Interest