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Broad (~10,000 km/s), double-peaked emission-line profiles of Balmer linesemitted by active galactic nuclei (AGN) are thought to originate in the outerparts of an accretion disk surrounding a nuclear supermassive black hole(SMBH), at R~1000 gravitational radii and are most frequently observed in thenuclear spectra of low-luminosity AGN (LLAGN) and radio-galaxies. In thepresent paper we argue that broad double-peaked profiles are present also inthe spectra of other Type 1 AGN, such as Seyfert 1 galaxies, suggesting thatthe inner part of the broad-line region (BLR) is also the outer part of theaccretion disk. We use the Palomar spectral survey of nearby galaxies to showthat the only difference between Seyfert 1 BLR line profiles and "bona fide"double peakers is that, in most cases, besides a disk component, we need anadditional Gaussian component attributed to non-disk clouds. The recognitionthat the inner and most variable part of the BLR has a disk geometry suggeststhat the factor 'f ' in the expression to obtain the SMBH mass (M) in Type 1AGN M(SMBH)=f [R(BLR) (Delta V)^2]/G is f = 1/[sin^2(i)] for the disk dominatedsources. Our median inclination i=27 degrees implies f=4.5, very close to themost recent value of f=4.3+/-1.05, obtained from independent studies. We derivea relation between f and the FWHM of the broad profile that may help to reducethe uncertainties in the SMBH mass determinations of AGN.

Double-peaked profiles: ubiquitous signatures of disks in the Broad Emission Lines of Active Galactic Nuclei