On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies

We investigate the relation between X-ray nuclear emission, optical emission line luminosities and black hole masses for a sample of 47 Seyfert galaxies. The sample, which has been selected from the Palomar optical spectroscopic survey of nearby galaxies ( Ho et al. 1997a, ApJS, 112, 315), covers a wide range of nuclear powers, from L2-10keV similar to 10(43) erg/s down to very low luminosities (L2-10 keV similar to 10(38) erg/s). Best available data from Chandra, XMM- Newton and, in a few cases, ASCA observations have been considered. Thanks to the good spatial resolution available from these observations and a proper modeling of the various spectral components, it has been possible to obtain accurate nuclear X-ray luminosities not contaminated by off-nuclear sources and/or diffuse emission. X-ray luminosities have then been corrected taking into account the likely candidate Compton thick sources, which are a high fraction (>= 30%) among type 2 Seyferts in our sample. The main result of this study is that we confirm strong linear correlations between 2 - 10 keV, [O-III]lambda 5007, H-alpha luminosities which show the same slope as quasars and luminous Seyfert galaxies, independent of the level of nuclear activity displayed. Moreover, despite the wide range of Eddington ratios (L/L-Edd) tested here ( six orders of magnitude, from 0.1 down to similar to 10(-7)), no correlation is found between the X-ray or optical emission line luminosities and the black hole mass. Our results suggest that Seyfert nuclei in our sample are consistent with being a scaled-down version of more luminous AGN.