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The direct detection of new extrasolar planets from high-precision photometrydata is commonly based on the observation of the transit signal of the planetas it passes in front of its star. Close-in planets, however, leave additionalimprints in the light curve even if they do not transit. These are theso-called phase curve variations that include ellipsoidal, reflection andbeaming effects. In Millholland & Laughlin (2017), the authors scrutinized theKepler database looking for these phase variations from non-transiting planets.They found 60 candidates whose signals were compatible with planetarycompanions. In this paper, we perform a ground-based follow-up of a sub-sampleof these systems with the aim of confirming and characterizing these planetsand thus validating the detection technique. We used the CAFE and HERMESinstruments to monitor the radial velocity of ten non-transiting planetcandidates along their orbits. We additionally used AstraLux to obtainhigh-resolution images of some of these candidates to discard blended binariesthat contaminate the Kepler light curves by mimicking planetary signals. Amongthe ten systems, we confirm three new hot-Jupiters (KIC8121913 b, KIC10068024b, and KIC5479689 b) with masses in the range 0.5-2 M$_{\rm Jup}$ and set massconstraints within the planetary regime for the other three candidates(KIC8026887b, KIC5878307 b, and KIC11362225 b), thus strongly suggestive oftheir planetary nature. For the first time, we validate the technique ofdetecting non-transiting planets via their phase curve variations. We presentthe new planetary systems and their properties. We find good agreement betweenthe RV-derived masses and the photometric masses in all cases except KIC8121913b, which shows a significantly lower mass derived from the ellipsoidalmodulations than from beaming and radial velocity data.

Follow-up of non-transiting planets detected by Kepler. Confirmation of three hot-Jupiters and validation of three other planets