  The hot Jupiter HD 217107 b was one of the first exoplanets detected using
the radial velocity (RV) method, originally reported in the literature in 1999.
Today, precise RV measurements of this system span more than 20 years, and
there is clear evidence for a longer-period companion, HD 217107 c.
Interestingly, both the short-period planet ($P_\mathrm{b}\sim7.13$ d) and
long-period planet ($P_\mathrm{c}\sim5059$ d) have significantly eccentric
orbits ($e_\mathrm{b}\sim0.13$ and $e_\mathrm{c}\sim0.40$). We present 42
additional RV measurements of this system obtained with the MINERVA telescope
array and carry out a joint analysis with previously published RV measurements
from four different facilities. We confirm and refine the previously reported
orbit of the long-period companion. HD 217107 b is one of a relatively small
number of hot Jupiters with an eccentric orbit, opening up the possibility of
detecting precession of the planetary orbit due to General Relativistic effects
and perturbations from other planets in the system. In this case, the argument
of periastron, $\omega$, is predicted to change at the level of
$\sim$0.8$^\circ$ century$^{-1}$. Despite the long time baseline of our
observations and the high quality of the RV measurements, we are only able to
constrain the precession to be $\dot{\omega}<65.9^\circ$ century$^{-1}$. We
discuss the limitations of detecting the subtle effects of precession in
exoplanet orbits using RV data.
