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As part of our radial velocity planet-search survey performed with SARG atTNG, we monitored the components of HD 132563 for ten years. It is a binarysystem formed by two rather similar solar type stars with a projectedseparation of 4.1 arcsec, which corresponds to 400 AU at the distance of 96 pc.The two components are moderately metal-poor and the age of the system is about5 Gyr. We detected RV variations of HD 132563B with period of 1544 days andsemi-amplitude of 26 m/s. From the star characteristics and line profilemeasurements, we infer their Keplerian origin. Therefore HD 132563B turns outto host a planet with a projected mass msini=1.49 MJup at 2.6 AU with amoderately eccentric orbit (e=0.22). The planet around HD 132563B is one of thefew that are known in triple stellar systems, as we found that the primary HD132563A is itself a spectroscopic binary with a period longer than 15 years andan eccentricity higher than 0.65. The spectroscopic component was not detectedin adaptive-optics images taken with AdOpt@TNG, since it expected at aprojected separation that was smaller than 0.2 arcsec at the time of ourobservations. A small excess in K band difference between the components withrespect to the difference in V band is compatible with a companion of about0.55 Msun. A preliminary statistical analysis of the occurrence of planets intriple systems indicate a similar frequency of planets around the isolatedcomponent in a triple system, components of wide binaries and single stars.There is no significant iron abundance difference between the components. Thelack of stars in binary systems and open clusters showing strong enhancementsof iron abundance, comparable to the typical metallicity difference betweenstars with and without giant planets, agrees with the idea that accretion ofplanetary material producing iron abundance anomalies larger than 0.1 dex israre.

A giant planet in the triple system HD132563