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HST/WFC3's spatial scan monitor automatically reduces and analyzestime-series data taken in spatial scan mode with the IR grisms. Here wedescribe the spatial scan monitor pipeline and present results derived fromeight years of transiting exoplanet data. Our goal is to monitor the quality ofthe data and make recommendations to users that will enhance futureobservations. We find that a typical observation achieves a white light curveprecision that is $1.07\times$ the photon-limit (which is slightly better thanexpectations) and that the pointing drift is relatively stable during times ofnormal telescope operations. We note that observations cannot achieve theoptimal precision when the drift along the dispersion direction ($X$ axis)exceeds 15 mas ($\sim$0.11 pixels). Based on our sample, 77.1% of observationsare ''successful'' ($<15$ mas rms drift), 12.0% are ''marginal'' (15 -- 135mas), and 10.8% of observations have ''failed'' ($>135$ mas or $>1$ pixel),meaning they do not achieve the necessary pointing stability to achieve theoptimal spectroscopic precision. In comparing the observed versus calculatedmaximum pixel fluence, we find that the J band is a better predictor of fluencethan the H band. Using this information, we derive an updated, empiricalrelation for scan rate that also accounts for the J-H color of the host star.We implement this relation and other improvements in version 1.4 of PandExo andversion 0.5 of ExoCTK. Finally, we make recommendations on how to plan futureobservations with increased precision.

Analyzing Eight Years of Transiting Exoplanet Observations Using WFC3's Spatial Scan Monitor