  We present a systematic investigation of the circumgalactic medium (CGM)
within projected distances d<160 kpc of luminous red galaxies (LRGs). The
sample comprises 16 intermediate-redshift (z=0.21-0.55) LRGs of stellar mass
M_star>1e11 M_sun. Combining far-ultraviolet Cosmic Origin Spectrograph spectra
from the Hubble Space Telescope and optical echelle spectra from the ground
enables a detailed ionization analysis based on resolved component structures
of a suite of absorption transitions, including the full HI Lyman series and
various ionic metal transitions. By comparing the relative abundances of
different ions in individually-matched components, we show that cool gas (T~1e4
K) density and metallicity can vary by more than a factor of ten in in an LRG
halo. Specifically, metal-poor absorbing components with <1/10 solar
metallicity are seen in 50% of the LRG halos, while gas with solar and
super-solar metallicity is also common. These results indicate a complex
multiphase structure and poor chemical mixing in these quiescent halos. We
calculate the total surface mass density of cool gas, \Sigma_cool, by applying
the estimated ionization fraction corrections to the observed HI column
densities. The radial profile of \Sigma_cool is best-described by a projected
Einasto profile of slope \alpha=1 and scale radius r_s=48 kpc. We find that
typical LRGs at z~0.4 contain cool gas mass of M_cool= (1-2) x1e10 M_sun at
d<160 kpc (or as much as 4x1e10 M_sun at d<500 kpc), comparable to the cool CGM
mass of star-forming galaxies. Furthermore, we show that high-ionization OVI
and low-ionization absorption species exhibit distinct velocity profiles,
highlighting their different physical origins. We discuss the implications of
our findings for the origin and fate of cool gas in LRG halos.
