  The nearby (6.5 pc) star HD 219134 was recently shown by Motalebi et al.
(2015) and Vogt et al. (2015) to host several planets, the innermost of which
is transiting. We present twenty-seven years of radial velocity observations of
this star from the McDonald Observatory Planet Search program, and nineteen
years of stellar activity data. We detect a long-period activity cycle measured
in the Ca II $S_{HK}$ index, with a period of $4230 \pm 100$ days (11.7 years),
very similar to the 11-year Solar activity cycle. Although the period of the
Saturn-mass planet HD 219134 h is close to half that of the activity cycle, we
argue that it is not an artifact due to stellar activity. We also find a
significant periodicity in the $S_{HK}$ data due to stellar rotation with a
period of 22.8 days. This is identical to the period of planet f identified by
Vogt et al. (2015), suggesting that this radial velocity signal might be caused
by rotational modulation of stellar activity rather than a planet. Analysis of
our radial velocities allows us to detect the long-period planet HD 219134 h
and the transiting super-Earth HD 219134 b. Finally, we use our long time
baseline to constrain the presence of longer-period planets in the system,
excluding to $1\sigma$ objects with $M\sin i>0.36 M_J$ at 12 years
(corresponding to the orbital period of Jupiter) and $M\sin i>0.72 M_J$ at a
period of 16.4 years (assuming a circular orbit for an outer companion).
