Measuring supermassive black holes with gas kinematics: the active S0 galaxy NGC 3998

We present results from a kinematical study of the gas in the nucleus of the active S0 galaxy NGC 3998 obtained from archival HST/STIS long-slit spectra. We analyzed the emission lines profiles and derived the map of the gas velocity field. The observed velocity curves are consistent with gas in regular rotation around the galaxy's center. By modeling the surface brightness distribution and rotation curve of the H_alfa emission line we found that the observed kinematics of the circumnuclear gas can be accurately reproduced by adding to the stellar mass component a compact dark mass (black hole) of M_bh = 2.7(-2.0,+2.4) 10**8 M_sun (uncertainties at a 2 sigma level); the radius of its sphere of influence (R_sph ~ 0".16) is well resolved at the HST resolution. The BH mass estimate in NGC 3998 is in good agreement with both the M_bh vs. M_bul (with an upward scatter by a factor of ~2) and M_bh vs. sigma correlations (with a downward scatter by a factor of ~3-7, depending on the form adopted for the dependence of M_bh on sigma). Although NGC 3998 cannot be considered as an outlier, its location with respect to the M_bh-sigma relation conforms with the trend suggesting the presence of a connection between the ``residuals'' from the M_bh-sigma correlation and the galaxy's effective radius. In fact, NGC 3998 has one of the smallest values of R_e among the galaxies with measured M_bh (0.85 kpc) and it shows a negative residual. This suggests that a combination of both sigma and R_e is necessary to drive the correlations between M_bh and other bulge properties, an indication for the presence of a black holes ``fundamental plane''