Resolving the inner accretion flow towards the central supermassive black hole in SDSS J1339+1310

Abstract

We studied the accretion disc structure in the doubly imaged lensed quasar SDSS J1339+1310 using $r$-band light curves and UV-visible to near-IR (NIR) spectra from the first 11 observational seasons after its discovery. The 2009$-$2019 light curves displayed pronounced microlensing variations on different timescales, and this microlensing signal permitted us to constrain the half-light radius of the 1930 Å continuum-emitting region. Assuming an accretion disc with an axis inclined at 60 deg to the line of sight, we obtained log${}_{10}$($r_{1/2}$/cm) = 15.4${}_{-0.4}^{+0.3}$. We also estimated the central black hole mass from spectroscopic data. The width of the Civ, Mgii, and H$\beta$ emission lines, and the continuum luminosity at 1350, 3000, and 5100 Å, led to log${}_{10}$($M_{BH}$/M${}_{\odot }$) = 8.6 $\pm$ 0.4. Thus, hot gas responsible for the 1930 Å continuum emission is likely orbiting a 4.0 $\times$ 10${}^8$ M${}_{\odot }$ black hole at an $r_{1/2}$ of only a few tens of Schwarzschild radii.

arXiv commentAccepted to A&A; 11 pages, 3 long tables (Tables 1 and 3-4) are available at the CDS

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