  The multiphase CGM hosts critical processes that affect galaxy evolution such
as accretion and outflows. We searched for evidence of these phenomena by using
the EW co-rotation fraction ($f_{\rm EWcorot}$) to study the kinematic
connection between the multiphase CGM and host galaxy rotation. We examined 27
systems with absorption lines from HST/COS (including, but not limited to,
SiII, CII, SiIII, CIII, and OVI) within $21\leq D\leq~276$ kpc of galaxies. We
find the median $f_{\rm EWcorot}$ for all ions is consistent within errors and
the $f_{\rm EWcorot}$ increases with increasing N$(\rm HI)$. The $f_{\rm
EWcorot}$ of lower ionization gas likely decreases with increasing $D/R_{\rm
vir}$ while OVI and HI are more consistent with being flat. The $f_{\rm
EWcorot}$ varies minimally as a function of azimuthal angle and is similar for
all ions at a fixed azimuthal angle. The larger number of OVI detections
enabled us to investigate where the majority of co-rotating gas is found.
Highly co-rotating OVI primarily resides along the galaxies' major axis.
Looking at the $f_{\rm EWcorot}$ as a function of ionization potential
(${d{f_{\rm EWcorot}}}/{d{(eV)}}$), we find a stronger co-rotation signature
for lower-ionization gas. There are suggestions of a connection between the CGM
metallicity and major axis co-rotation where low-ionization gas with higher
$f_{\rm EWcorot}$ exhibits lower metallicity and may trace large-scale
filamentary inflows. Higher ionization gas with higher $f_{\rm EWcorot}$
exhibits higher metallicity and may instead trace co-planar recycled gas
accretion. Our results stress the importance of comparing absorption
originating from a range of ionization phases to differentiate between various
gas flow scenarios.
