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In the letter, under the widely accepted theoretical accretion disk model forthe double-peaked emitter 3C390.3, the extended disk-like BLR can be well splitinto ten rings, and then the time lags between the lines from the rings and thecontinuum emission are estimated, based on the observed spectra around 1995. Wecan find one much strong correlation between the determined time lags (in unitof light-day) and the flux weighted radii (in unit of ${\rm R_G}$) of therings, which is well consistent with the expected results through thetheoretical accretion disk model. Moreover, through the strong correlation, theblack hole masses of 3C390.3 are independently estimated as $\sim10^9{\rmM_{\odot}}$, the same as the reported black hole masses in the literature. Theconsistencies provide further evidence to strongly support the accretion diskorigination of the double-peaked broad balmer lines of 3C390.3.

Further Evidence for the Accretion Disk Origination of the Double-Peaked Broad H$\alpha$ of 3C390.3