As part of our radial velocity planet-search survey performed with SARG at TNG , we monitored the components of HD 132563 for ten years .
It is a binary system formed by two rather similar solar type stars with a projected separation of 4.1 arcsec , which corresponds to 400 AU at the distance of 96 pc .
The two components are moderately metal-poor ( [ Fe/H ] =–0.19 ) , and the age of the system is about 5 Gyr .
We detected RV variations of HD 132563B with period of 1544 days and semi-amplitude of 26 m/s .
From the star characteristics and line profile measurements , we infer their Keplerian origin .
Therefore HD 132563B turns out to host a planet with a projected mass m \sin i = 1.49 ~ { } M _ { J } at 2.6 AU with a moderately eccentric orbit ( e = 0.22 ) .
The planet around HD 132563B is one of the few that are known in triple stellar systems , as we found that the primary HD 132563A is itself a spectroscopic binary with a period longer than 15 years and an eccentricity higher than 0.65 .
The spectroscopic component was not detected in adaptive-optics images taken with AdOpt @ TNG , since it expected at a projected separation that was smaller than 0.2 arcsec at the time of our observations .
A small excess in K band difference between the components with respect to the difference in V band is compatible with a companion of about 0.55 ~ { } M { { } _ { \odot } } .
A preliminary statistical analysis of when planets occur in triple systems indicate a similar frequency of planets around the isolated component in a triple system , components of wide binaries and single stars .
There is no significant iron abundance difference between the components ( \Delta [ Fe/H ] = 0.012 \pm 0.013 dex ) .
The lack of stars in binary systems and open clusters showing strong enhancements of iron abundance , which are comparable to the typical metallicity difference between stars with and without giant planets , agrees with the idea that accretion of planetary material producing iron abundance anomalies over 0.1 dex is rare .