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Accurately weigh the masses of SMBH in AGN is currently possible for only asmall group of local and bright broad-line AGN through reverberation mapping(RM). Statistical demographic studies can be carried out considering theempirical scaling relation between the size of the BLR and the AGN opticalcontinuum luminosity. However, there are still biases against low-luminosity orreddened AGN, in which the rest-frame optical radiation can be severelyabsorbed/diluted by the host and the BLR emission lines could be hard todetect. Our purpose is to widen the applicability of virial-based SE relationsto reliably measure the BH masses also for low-luminosity or intermediate/type2 AGN that are missed by current methodology. We achieve this goal bycalibrating virial relations based on unbiased quantities: the hard X-rayluminosities, in the 2-10 keV and 14-195 keV bands, that are less sensitive togalaxy contamination, and the FWHM of the most important rest-frame NIR andoptical BLR emission lines. We built a sample of RM AGN having both X-rayluminosity and broad optical/NIR FWHM measurements available in order tocalibrate new virial BH mass estimators. We found that the FWHM of theH$\alpha$, H$\beta$ and NIR lines (i.e. Pa$\alpha$, Pa$\beta$ andHeI$\lambda$10830) all correlate each other having negligible or small offsets.This result allowed us to derive virial BH mass estimators based on either the2-10 keV or 14-195 keV luminosity. We took also into account the recentdetermination of the different virial coefficients $f$ for pseudo and classicalbulges. By splitting the sample according to the bulge type and adoptingseparate $f$ factors we found that our virial relations predict BH masses ofAGN hosted in pseudobulges $\sim$0.5 dex smaller than in classical bulges.Assuming the same average $f$ factor for both populations, a difference of$\sim$0.2 dex is still found.

Novel calibrations of virial black hole mass estimators in active galaxies based on X-ray luminosity and optical/NIR emission lines