Resolving the inner accretion flow towards the central supermassive black hole in SDSS J1339+1310
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 tim...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2021 |
| País: | España |
| Institución: | Universidad de Cantabria (UC) |
| Repositorio: | UCrea Repositorio Abierto de la Universidad de Cantabria |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unican.es:10902/24778 |
| Acceso en línea: | http://hdl.handle.net/10902/24778 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion, accretion disks Gravitational lensing: micro Gravitational lensing: strong Quasars: individual: SDSS J1339+1310 Quasars: supermassive black hole |
| Sumario: | 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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