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$\textit{Swift}$'s rapid slewing, flexible planning, and multi-wavelengthinstruments make it the most capable space-based follow-up engine for findingpoorly localized sources. During O1 and O2 $\textit{Swift}$ successfully tiledhundreds of square-degrees of sky in the LVC localization regions, searchingfor, and identifying, possible X-ray and UV/O transients in the field.$\textit{Swift}$ made important contributions to the discovery andcharacterization of the kilonova AT 2017gfo, discovering the UV emission andproviding the deepest X-ray upper limits in the first 24 hours after thetrigger, strongly constraining the dynamics and geometry of the counterpart.$\textit{Swift}$ tiled 92% of the galaxy convolved error region down to averageX-ray flux sensitivities of $10^{-12}$ erg $\mbox{cm}^{-2}$ $\mbox{s}^{-1}$,significantly increasing our confidence that AT 2017gfo is indeed thecounterpart to GW 170817 and sGRB 170817. However, there remains significantroom for improvement of $\textit{Swift}$'s follow-up in preparation for O3.This will take the form of both revised observation strategy based on detailedanalysis of the results from O2, and significant changes to $\textit{Swift}$'soperational capabilities. These improvements are necessary both for maximizingthe likelihood that $\textit{Swift}$ finds a counterpart, and minimizing theimpact that follow-up activities have on other $\textit{Swift}$ sciencepriorities. We outline areas of improvement to the observing strategy itselffor optimal tiling of the LVC localization regions. We also discuss ongoingwork on operational upgrades that will decrease latency in our response time,and minimize impact on pre-planned observations, while maintaining spacecrafthealth and safety.

GW170817: $\textit{Swift}$ UV detection of a blue kilonova, and improving the search in O3