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Precision radial velocities are required to discover and characterize planetsorbiting nearby stars. Optical and near infrared spectra that exhibit manyhundreds of absorption lines can allow the m/s precision levels required forsuch work. However, this means that studies have generally focused onsolar-type dwarf stars. After the main-sequence, intermediate-mass stars(former A-F stars) expand and rotate slower than their progenitors, thusthousands of narrow absorption lines appear in the optical region, permittingthe search for planetary Doppler signals in the data for these types of stars.We present the discovery of two giant planets around the intermediate-massevolved star HIP65891 and HIP107773. The best Keplerian fit to the HIP65891 andHIP107773 radial velocities leads to the following orbital parameters: P=1084.5d; m$_b$sin$i$ = 6.0 M$_{jup}$; $e$=0.13 and P=144.3 d; m$_b$sin$i$ = 2.0M$_{jup}$; $e$=0.09, respectively. In addition, we confirm the planetary natureof the outer object orbiting the giant star HIP67851. The orbital parameters ofHIP67851c are: P=2131.8 d, m$_c$sin$i$ = 6.0 M$_{jup}$ and $e$=0.17. Withmasses of 2.5 M$_\odot$ and 2.4 M$_\odot$ HIP65891 and HIP107773 are two of themost massive stars known to host planets. Additionally, HIP67851 is one of fivegiant stars that are known to host a planetary system having a close-in planet($a <$ 0.7 AU). Based on the evolutionary states of those five stars, weconclude that close-in planets do exist in multiple systems around subgiantsand slightly evolved giants stars, but probably they are subsequently destroyedby the stellar envelope during the ascent of the red giant branch phase. As aconsequence, planetary systems with close-in objects are not found aroundhorizontal branch stars.

Giant planets around two intermediate-mass evolved stars and confirmation of the planetary nature of HIP67851 c