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

The multiphase circumgalactic medium (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 () to study the kinematic connection between the multiphase CGM and host galaxy rotation. We examined CGM absorption from Hubble Space Telescope /Cosmic Origins Spectrograph (including, but not limited to, Si ii, C ii, Si iii, C iii, and O vi) within kpc of 27 galaxies. We find the median for all ions is consistent within errors and the increases with increasing N. The of lower ionization gas decreases with increasing, while O vi and H i are consistent with being flat. The varies minimally as a function of azimuthal angle and is similar for all ions at a fixed azimuthal angle. The larger number of O vi detections enabled us to investigate where the majority of co-rotating gas is found. Highly co-rotating O vi primarily resides along the galaxies' major axis. Looking at the as a function of ionization potential (), 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 exhibits lower metallicity and may trace large-scale filamentary inflows. Higher ionization gas with higher 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.