  We study ultraviolet HI and metal line transitions in the circumgalactic
medium (CGM) of 15 massive, quenched luminous red galaxies (LRGs) at redshift
$z\sim 0.5$ and with impact parameters up to 400 kpc. We selected 8 of LRG-CGM
systems to study general properties of the CGM around LRGs, while the other 7
are already known to contain cool CGM gas from MgII optical studies
(MgII-LRGs). In the general LRGs population, we detect HI in 4 of 8 LRGs, in
all cases with $N_{HI} < 10^{16.7} {\rm cm^{-2}}$. In contrast, all MgII-LRGs
show HI; for four LRGs the HI column density is $N_{HI} \gtrsim 10^{18} {\rm
cm^{-2}}$. The CGM of LRGs also shows low and intermediate ionized lines (such
as CIII, CII, SiIII, SiII) and highly ionized lines of OVI (we detect OVI
around 5 of 7 MgII-LRGs and 1 of 8 in the random sample). Next, we combine our
sample with literature LRGs and $\lesssim L^{*}$ galaxies and we find that
while for $\lesssim L^{*}$ galaxies CGM HI Ly$\alpha$ absorption is stronger as
galaxies are more massive, the cool CGM traced by HI Ly$\alpha$ is suppressed
above stellar masses of $M* \sim 10^{11.5}$ $M_{\odot}$. While most LRG CGM
systems show weak or non-detectable OVI (equivalent width less than 0.2 \AA), a
few LRG CGM systems show strong OVI 1031, which in most cases likely originates
from groups containing both a LRG and a blue star-forming neighboring galaxy.
