  We analyzed the microlensing of the X-ray and optical emission of the lensed
quasar PG 1115+080. We find that the effective radius of the X-ray emission is
1.3(+1.1 -0.5) dex smaller than that of the optical emission. Viewed as a thin
disk observed at inclination angle i, the optical accretion disk has a scale
length, defined by the point where the disk temperature matches the rest frame
energy of the monitoring band (kT=hc/lambda_rest with lambda_rest=0.3 micron),
of log[(r_{s,opt}/cm)(cos(i) / 0.5)^{1/2}] = 16.6 \pm 0.4. The X-ray emission
region (1.4-21.8 keV in the rest frame) has an effective half-light radius of
log[r_{1/2,X}/cm] = 15.6 (+0.6-0.9}. Given an estimated black hole mass of 1.2
* 10^9 M_sun, corresponding to a gravitational radius of log[r_g/cm] = 14.3,
the X-ray emission is generated near the inner edge of the disk while the
optical emission comes from scales slightly larger than those expected for an
Eddington-limited thin disk. We find a weak trend supporting models with low
stellar mass fractions near the lensed images, in mild contradiction to
inferences from the stellar velocity dispersion and the time delays.
