Accretion Onto the Supermassive Black Hole in the High-redshift Radio-loud AGN 0957+561

Details Accretion Onto the Supermassive Black Hole in the High-redshift Radio-loud AGN 0957+561 Accretion Onto the Supermassive Black Hole in the High-redshift Radio-loud AGN 0957+561

2011-09-15

arxiv.org/abs/1109.3330v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

21 pages, 7 text pages, 13 figures, 2 tables, accepted by The Astrophysical Journal

Scientific paper

We present the results of our X-ray, UV and optical monitoring campaign of the first gravitationally lensed AGN from late 2009 to mid 2010. The trailing (B) image of the AGN 0957+561 shows the intrinsic continuum variations that were predicted in advance based on observations of the leading (A) image in the gr optical bands. This multiwavelength variability of the B image allows us to carry out a reverberation mapping analysis in the radio-loud AGN 0957+561 at redshift z = 1.41. We find that the U-band and r-band light curves are highly correlated with the g-band record, leading and trailing it by 3 +/- 1 days (U band) and 4 +/- 1 days (r band). These 1-sigma measurements are consistent with a scenario in which flares originated in the immediate vicinity of the supermassive black hole are thermally reprocessed in a standard accretion disk at about 10-20 Schwarzschild radii from the central dark object. We also report that the light curve for the X-ray emission with power-law spectrum is delayed with respect to those in the Ugr bands by about 32 days. Hence, the central driving source can not be a standard corona emitting the observed power-law X-rays. This result is also supported by X-ray reprocessing simulations and the absence of X-ray reflection features in the spectrum of 0957+561. We plausibly interpret the lack of reflection and the 32-day delay as evidence for a power-law X-ray source in the base of the jet at a typical height of about 200 Schwarzschild radii. A central EUV source would drive the variability of 0957+561.

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