Resolving the inner accretion flow towards the central supermassive black hole in SDSS J1339+1310
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Shalyapin, Vyacheslav; Goicoechea Santamaría, Luis Julián; Morgan, C. W.; Cornachione, M. A.; Sergeyev, A. V.Fecha
2021Derechos
© ESO
Publicado en
Astronomy & Astrophysics. Vol. 646, February 2021. A165
Editorial
EDP Sciences
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Palabras clave
Accretion, accretion disks
Gravitational lensing: micro
Gravitational lensing: strong
Quasars: individual: SDSS J1339+1310
Quasars: supermassive black hole
Resumen/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 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° to the line of sight, we obtained log(r1/2/cm) = 15.4−0.4+0.93. We also estimated the central black hole mass from spectroscopic data. The width of the C IV, Mg II, and Hβ emission lines, and the continuum luminosity at 1350, 3000, and 5100 Å, led to log(MBH/M⊙) = 8.6 ± 0.4. Thus, hot gas responsible for the 1930 Å continuum emission is likely orbiting a 4.0 × 108 M⊙ black hole at an r1/2 of only a few tens of Schwarzschild radii.
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