Strong Chromatic Microlensing in HE0047-1756 and SDSS1155+6346

Abstract

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${}_s^2$)) 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.

31 pages, 7 figures, 7 tables. Accepted for publication in ApJ

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