English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We use spectra of the double lensed quasars HE0047-1756 and SDSS1155+6346 tostudy their unresolved structure through the impact of microlensing. There isno significant evidence of microlensing in the emission line profiles exceptfor the Ly$\alpha$ line of SDSS1155+6346, which shows strong differences in theshapes for images A and B. However, the continuum of the B image spectrum inSDSS1155+6346 is strongly contaminated by the lens galaxy and these differencesshould be considered with caution. Using the flux ratios of the emission linesfor image pairs as a baseline to remove macro-magnification and extinction, wehave detected strong chromatic microlensing in the continuum measured byCASTLES (http://www.cfa.harvard.edu/castles/), in both lens systems, withamplitudes $0.09 (\lambda 16000) \lesssim |\Delta m |\lesssim 0.8 (\lambda5439)$ for HE0047-1756, and $0.2 (\lambda 16000) \lesssim |\Delta m |\lesssim0.8 (\lambda 5439)$ for SDSS1155+6346. Using magnification maps to simulatemicrolensing, 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 (logprior). Contrary to other studied lens systems, the chromaticity detected inHE0047-1756 and SDSS1155+6346 is large enough to fulfill the thin diskprediction. The inferred sizes, however, are very large compared to thepredictions of this model, especially in the case of SDSS1155+6346.

Strong Chromatic Microlensing in HE0047-1756 and SDSS1155+6346