  $\textit{Swift}$'s rapid slewing, flexible planning, and multi-wavelength
instruments make it the most capable space-based follow-up engine for finding
poorly localized sources. During O1 and O2 $\textit{Swift}$ successfully tiled
hundreds of square-degrees of sky in the LVC localization regions, searching
for, and identifying, possible X-ray and UV/O transients in the field.
$\textit{Swift}$ made important contributions to the discovery and
characterization of the kilonova AT 2017gfo, discovering the UV emission and
providing the deepest X-ray upper limits in the first 24 hours after the
trigger, strongly constraining the dynamics and geometry of the counterpart.
$\textit{Swift}$ tiled 92% of the galaxy convolved error region down to average
X-ray flux sensitivities of $10^{-12}$ erg $\mbox{cm}^{-2}$ $\mbox{s}^{-1}$,
significantly increasing our confidence that AT 2017gfo is indeed the
counterpart to GW 170817 and sGRB 170817. However, there remains significant
room for improvement of $\textit{Swift}$'s follow-up in preparation for O3.
This will take the form of both revised observation strategy based on detailed
analysis of the results from O2, and significant changes to $\textit{Swift}$'s
operational capabilities. These improvements are necessary both for maximizing
the likelihood that $\textit{Swift}$ finds a counterpart, and minimizing the
impact that follow-up activities have on other $\textit{Swift}$ science
priorities. We outline areas of improvement to the observing strategy itself
for optimal tiling of the LVC localization regions. We also discuss ongoing
work on operational upgrades that will decrease latency in our response time,
and minimize impact on pre-planned observations, while maintaining spacecraft
health and safety.
