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

V. N. Shalyapin; L. J. Goicoechea; C. W. Morgan; M. A. Cornachione; A. V. Sergeyev

doi:10.1051/0004-6361/202038770

paper

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

arXiv:2101.01116 · doi:10.1051/0004-6361/202038770

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 $β$ emission lines, and the continuum luminosity at 1350, 3000, and 5100 Å, led to log $_{10}$ ( $M_{B H}$ /M $_{⊙}$ ) = 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 $_{⊙}$ black hole at an $r_{1/2}$ of only a few tens of Schwarzschild radii.

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

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

Abstract

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