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The multiphase CGM hosts critical processes that affect galaxy evolution suchas accretion and outflows. We searched for evidence of these phenomena by usingthe EW co-rotation fraction ($f_{\rm EWcorot}$) to study the kinematicconnection between the multiphase CGM and host galaxy rotation. We examined 27systems 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. Wefind the median $f_{\rm EWcorot}$ for all ions is consistent within errors andthe $f_{\rm EWcorot}$ increases with increasing N$(\rm HI)$. The $f_{\rmEWcorot}$ of lower ionization gas likely decreases with increasing $D/R_{\rmvir}$ while OVI and HI are more consistent with being flat. The $f_{\rmEWcorot}$ varies minimally as a function of azimuthal angle and is similar forall ions at a fixed azimuthal angle. The larger number of OVI detectionsenabled 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 signaturefor lower-ionization gas. There are suggestions of a connection between the CGMmetallicity and major axis co-rotation where low-ionization gas with higher$f_{\rm EWcorot}$ exhibits lower metallicity and may trace large-scalefilamentary inflows. Higher ionization gas with higher $f_{\rm EWcorot}$exhibits higher metallicity and may instead trace co-planar recycled gasaccretion. Our results stress the importance of comparing absorptionoriginating from a range of ionization phases to differentiate between variousgas flow scenarios.

Signatures of gas flows-II: Connecting the kinematics of the multiphase circumgalactic medium to galaxy rotation