  We analyze the cool gas in and around 14 nearby galaxies (at $z$$<$0.1)
mapped with the SDSS-IV MaNGA survey by measuring absorption lines produced by
gas in spectra of background quasars/AGN at impact parameters of 0-25 effective
radii from the galaxy center. Using HST/COS, we detect absorption at the galaxy
redshift and measure or constrain column densities of neutral (H I, N I, O I,
Ar I), low-ionization (Si II, S II, C II, N II Fe II), and high-ionization (Si
III, Fe III, N V, O VI) species for 11 galaxies. We derive the ionization
parameter and ionization-corrected metallicity using CLOUDY photo-ionization
models. The H I column density ranges from $\sim$$10^{13}$ to
$\sim$$10^{20}\,{\rm cm^{-2}}$ and decreases with impact parameter for $r \ge
R_{e}$. Galaxies with higher stellar mass have weaker H I absorption. Comparing
absorption velocities with MaNGA radial velocity maps of ionized gas line
emissions in galactic disks, we find that the neutral gas seen in absorption
co-rotates with the disk out to $\sim$10 $R_{e}$. Sight lines with lower
elevation angles show lower metallicities, consistent with the metallicity
gradient in the disk derived from MaNGA maps. Higher elevation angle sight
lines show higher ionization, lower H I-column density, super-solar
metallicity, and velocities consistent with the direction of galactic outflow.
Our data offer the first detailed comparisons of CGM properties (kinematics and
metallicity) with extrapolations of detailed galaxy maps from integral field
spectroscopy; similar studies for larger samples are needed to more fully
understand how galaxies interact with their CGM.
