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We present results from a kinematical study of the gas in the nucleus of asample of three LINER galaxies, obtained from archival HST/STIS long-slitspectra. We found that, while for the elliptical galaxy NGC 5077, the observedvelocity curves are consistent with gas in regular rotation around the galaxy'scenter, this is not the case for the two remaining objects. By modeling thesurface brightness distribution and rotation curve from the emission lines inNGC 5077, we found that the observed kinematics of the circumnuclear gas can beaccurately reproduced by adding to the stellar mass component a black hole massof M_bh = 6.8 (-2.8,+4.3) 10**8 M_sun (uncertainties at a 1 sigma level); theradius of its sphere of influence (R_sph ~ 0".34) is well-resolved at the HSTresolution. The BH mass estimate in NGC 5077 is in fairly good agreement withboth the M_bh-M_bul (with an upward scatter of ~ 0.4 dex) and M_bh-sigmacorrelations (with an upward scatter of 0.5 dex in the Tremaine et al. form andessentially no scatter using the Ferrarese et al. form) and provides furthersupport for the presence of a connection between the ``residuals'' from theM_bh-sigma correlation and the bulge effective radius. This indicates thepresence of a black hole's ``fundamental plane'' in the sense that acombination of at least sigma and R_e drives the correlations between M_bh andhost bulge properties.

Measuring supermassive black holes with gas kinematics - II. The LINERs IC 989, NGC 5077, and NGC 6500