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Microlensing has proven an effective probe of the structure of the innermostregions of quasars, and an important test of accretion disk models. We presentlight curves of the lensed quasar HE 0435-1223 in the R band and in theultraviolet, and consider them together with X-ray light curves in two energybands that are presented in a companion paper. Using a Bayesian Monte Carlomethod, we constrain the size of the accretion disk in the rest-frame near- andfar-UV, and constrain for the first time the size of the X-ray emission regionsin two X-ray energy bands. The R-band scale size of the accretion disk is about10^15.23 cm (~23 r_g), slightly smaller than previous estimates, but largerthan would be predicted from the quasar flux. In the UV, the source size isweakly constrained, with a strong prior dependence. The UV to R-band size ratiois consistent with the thin disk model prediction, with large error bars. Insoft and hard X-rays, the source size is smaller than ~10^14.8 cm (~10 r_g) at95% confidence. We do not find evidence of structure in the X-ray emissionregion, as the most likely value for the ratio of the hard X-ray size to thesoft X-ray size is unity. Finally, we find that the most likely value for themean mass of stars in the lens galaxy is ~0.3 M_sun, consistent with otherstudies.

The Optical, Ultraviolet, and X-ray Structure of the Quasar HE 0435-1223