Accretion disk and wind emission in the Population B, jetted quasar 3C 47

An optically thick, geometrically thin accretion disk around a supermassive black hole might contribute to broad line emission

in type-1 active galactic nuclei (AGN). We show that the double-peaked profiles of the strongest low-ionization lines

(LILs) in the 3C 47 optical spectrum can be explained by a relativistic Keplerian accretion disk model. The profiles of

prototypical high ionization lines (HILs) such as CIVλ1549 were also modeled by the contribution of the accretion

disk, but required an additional component, possibly due to a failed wind. The observations of 3C 47 suggest an

intriguing hypothesis for the origin of the “double-peakers,” sources found at the low end of radiative power per unit

black hole mass along the quasar main sequence.