  A historical problem for indirect exoplanet detection has been contending
with the intrinsic variability of the host star. If the variability is
periodic, it can easily mimic various exoplanet signatures, such as radial
velocity variations that originate with the stellar surface rather than the
presence of a planet. Here we present an update for the HD~99492 planetary
system, using new radial velocity and photometric measurements from the Transit
Ephemeris Refinement and Monitoring Survey (TERMS). Our extended time series
and subsequent analyses of the Ca II H\&K emission lines show that the host
star has an activity cycle of $\sim$13 years. The activity cycle correlates
with the purported orbital period of the outer planet, the signature of which
is thus likely due to the host star activity. We further include a revised
Keplerian orbital solution for the remaining planet, along with a new transit
ephemeris. Our transit-search observations were inconclusive.
