  We study the dependence of quasar clustering on quasar luminosity and black
hole mass by measuring the angular overdensity of photometrically selected
galaxies imaged by WISE about z $\sim$ 0.8 quasars from SDSS. By measuring the
quasar-galaxy cross-correlation function and using photometrically selected
galaxies, we achieve a higher density of tracer objects and a more sensitive
detection of clustering than measurements of the quasar autocorrelation
function. We test models of quasar formation and evolution by measuring the
luminosity dependence of clustering amplitude. We find a significant
overdensity of WISE galaxies about z $\sim$ 0.8 quasars at 0.2--6.4 h$^{-1}$
Mpc in projected comoving separation. We find no appreciable increase in
clustering amplitude with quasar luminosity across a decade in luminosity, and
a power-law fit between luminosity and clustering amplitude gives an exponent
of $-$0.01 $\pm$ 0.06 (1 $\sigma$ errorbar). We also fail to find a significant
relationship between clustering amplitude and black hole mass, although our
dynamic range in true mass is suppressed due to the large uncertainties in
virial black hole mass estimates. Our results indicate that a small range in
host dark matter halo mass maps to a large range in quasar luminosity.
