  We use spectra of the double lensed quasars HE0047-1756 and SDSS1155+6346 to
study their unresolved structure through the impact of microlensing. There is
no significant evidence of microlensing in the emission line profiles except
for the Ly$\alpha$ line of SDSS1155+6346, which shows strong differences in the
shapes for images A and B. However, the continuum of the B image spectrum in
SDSS1155+6346 is strongly contaminated by the lens galaxy and these differences
should be considered with caution. Using the flux ratios of the emission lines
for image pairs as a baseline to remove macro-magnification and extinction, we
have detected strong chromatic microlensing in the continuum measured by
CASTLES (http://www.cfa.harvard.edu/castles/), in both lens systems, with
amplitudes $0.09 (\lambda 16000) \lesssim |\Delta m |\lesssim 0.8 (\lambda
5439)$ for HE0047-1756, and $0.2 (\lambda 16000) \lesssim |\Delta m |\lesssim
0.8 (\lambda 5439)$ for SDSS1155+6346. Using magnification maps to simulate
microlensing, and modeling the accretion disk as a Gaussian source (I $\propto$
exp(-R$^{2}$/2r$^2_s$)) of size r$_{s}$ $\propto$ $ \lambda^{p} $ we find,
r$_{s}$ = 2.5$_{-1.4}^{+3.0}$ $\sqrt{M/0.3M_{\odot}}$ light days and p = 2.3
$\pm$ 0.8, at the rest frame for $\lambda$ = 2045, for HE0047-1756 (log prior),
and r$_{s}$ = 5.5$_{-3.3}^{+8.2}$ $\sqrt{M/0.3M_{\odot}}$ light days and p =
1.5 $\pm$ 0.6 at the rest frame of $\lambda$ = 1398, for SDSS1155+6346 (log
prior). Contrary to other studied lens systems, the chromaticity detected in
HE0047-1756 and SDSS1155+6346 is large enough to fulfill the thin disk
prediction. The inferred sizes, however, are very large compared to the
predictions of this model, especially in the case of SDSS1155+6346.
