  We report the detection of two new long-period giant planets orbiting the
stars HD 95872 and HD 162004 (psi1 Draconis B) by the McDonald Observatory
planet search. The planet HD 95872b has a minimum mass of 4.6 M_Jup and an
orbital semi-major axis of 5.2 AU. The giant planet psi1 Dra Bb has a minimum
mass of 1.5 M_Jup and an orbital semi-major axis of 4.4 AU. Both of these
planets qualify as Jupiter analogs. These results are based on over one and a
half decades of precise radial velocity measurements collected by our program
using the McDonald Observatory Tull Coude spectrograph at the 2.7 m Harlan J.
Smith telescope. In the case of psi1 Draconis B we also detect a long-term
non-linear trend in our data that indicates the presence of an additional giant
planet, similar to the Jupiter-Saturn pair. The primary of the binary star
system, psi1 Dra A, exhibits a very large amplitude radial velocity variation
due to another stellar companion. We detect this additional member using
speckle imaging. We also report two cases - HD 10086 and HD 102870 (beta
Virginis) - of significant radial velocity variation consistent with the
presence of a planet, but that are probably caused by stellar activity, rather
than reflexive Keplerian motion. These two cases stress the importance of
monitoring the magnetic activity level of a target star, as long-term activity
cycles can mimic the presence of a Jupiter-analog planet.
