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A historical problem for indirect exoplanet detection has been contendingwith the intrinsic variability of the host star. If the variability isperiodic, it can easily mimic various exoplanet signatures, such as radialvelocity variations that originate with the stellar surface rather than thepresence of a planet. Here we present an update for the HD~99492 planetarysystem, using new radial velocity and photometric measurements from the TransitEphemeris Refinement and Monitoring Survey (TERMS). Our extended time seriesand subsequent analyses of the Ca II H\&K emission lines show that the hoststar has an activity cycle of $\sim$13 years. The activity cycle correlateswith the purported orbital period of the outer planet, the signature of whichis thus likely due to the host star activity. We further include a revisedKeplerian orbital solution for the remaining planet, along with a new transitephemeris. Our transit-search observations were inconclusive.

Stellar Activity and Exclusion of the Outer Planet in the HD 99492 System