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BD+20 1790 is a young active, metal-rich, late-type K5Ve star. We haveundertaken a study of stellar activity and kinematics for this star over thepast few years. Previous results show a high level of stellar activity, withthe presence of prominence-like structures, spots on the surface and strongflare events, despite the moderate rotational velocity of the star. Inaddition, radial velocity variations with a semi-amplitude of up to 1 km/s weredetected. We investigated the nature of these radial velocity variations, inorder to determine whether they are due to stellar activity or the reflexmotion of the star induced by a companion. We have analysed high-resolutionechelle spectra and also two-band photometry was obtained to produce the lightcurve and determine the photometric period. Based upon the analysis of thebisector velocity span, as well as spectroscopic indices of chromosphericindicators and taking into account the photometric analysis, we report that thebest explanation for the RV variation is the presence of a sub-stellarcompanion. The Keplerian fit of the RV data yields a solution for a close-inmassive planet with an orbital period of 7.78 days. The presence of theclose-in massive planet could also be an interpretation for the high level ofstellar activity detected. Since the RV data are not part of a planet searchprogram, we can consider our results as a serendipitous evidence of a planetarycompanion. To date, this is the youngest main sequence star for which aplanetary candidate has been reported.

Evidence of a massive planet candidate orbiting the young active K5V star BD+20 1790