Context : Precision radial velocities are required to discover and characterize planets orbiting nearby stars .
Optical and near infrared spectra that exhibit many hundreds of absorption lines can allow the m s ^ { -1 } precision levels required for such work .
However , this means that studies have generally focused on solar-type dwarf stars .
After the main-sequence , intermediate-mass stars ( former A-F stars ) expand and rotate slower than their progenitors , thus thousands of narrow absorption lines appear in the optical region , permitting the search for planetary Doppler signals in the data for these types of stars .

Aims : In 2009 , we began the EXPRESS program , aimed at detecting substellar objects around evolved stars , and to study the effects of the mass and evolution of the host star on their orbital and physical properties .

Methods : We have obtained precision radial velocity measurements for the giant stars HIP 65891 and HIP 107773 , from CHIRON and FEROS spectra .
Also , we obtained new radial velocity epochs for the star HIP 67851 , which is known to host a planetary system .

Results : We present the discovery of two giant planets around the intermediate-mass evolved star HIP 65891 and HIP 107773 .
The best Keplerian fit to the HIP 65891 and HIP 107773 radial velocities leads to the following orbital parameters : P=1084.5 d ; m _ { b } sin i = 6.0 M _ { J } ; e =0.13 and P=144.3 d ; m _ { b } sin i = 2.0 M _ { J } ; e =0.09 , respectively .
In addition , we confirm the planetary nature of the outer object orbiting the giant star HIP 67851 .
The orbital parameters of HIP 67851 c are : P=2131.8 d , m _ { c } sin i = 6.0 M _ { J } and e =0.17 .

Conclusions : With masses of 2.5 M _ { \odot } and 2.4 M _ { \odot } , HIP 65891 and HIP 107773 are two of the most massive stars known to host planets .
Additionally , HIP 67851 is one of five giant 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 , we conclude that close-in planets do exist in multiple systems around subgiants and slightly evolved giants stars , but probably they are subsequently destroyed by the stellar envelope during the ascent of the red giant branch phase .
As a consequence , planetary systems with close-in objects are not found around horizontal branch stars .