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For over 10 years, we have carried out a precise radial velocity (RV) surveyto find substellar companions around evolved G,K-type stars to extend ourknowledge of planet formation and evolution. We performed high precision RVmeasurements for the giant star HD 208897 using an iodine (I2) absorption cell.The measurements were made at T\"UB\.ITAK National Observatory (TUG, RTT150)and Okayama Astrophysical Observatory (OAO). For the origin of the periodicvariation seen in the RV data of the star, we adopted a Keplerian motion causedby an unseen companion. We found that the star hosts a planet with a minimummass of m2sini=1.40MJ, which is relatively low compared to those of knownplanets orbiting evolved intermediate-mass stars. The planet is in a nearlycircular orbit with a period of P=353 days at about 1 AU distance from the hoststar. The star is metal rich and located at the early phase of ascent along thered giant branch. The photometric observations of the star at Ankara UniversityKreiken Observatory (AUKR) and the HIPPARCOS photometry show no sign ofvariation with periods associated with the RV variation. Neither bisectorvelocity analysis nor analysis of the Ca II and Halpha lines shows anycorrelation with the RV measurements.

A Jupiter-mass planet around the K0 giant HD 208897