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Narrow optical emission-line profiles representing a wide range in ionization potential for 12 high-ionization Seyfert galaxies are analyzed using deconvolution techniques. The data reduction process is described in detail. A good correlation is found between line width and ionization potential in many of the objects. For some galaxies a good correlation is also found between line width and critical density. For a given object, the ratios of line widths at various fractions of full intensity are remarkably similar over the entire range of ionization potential and critical density. Almost identical velocity ratios at corresponding fractions of maximum intensity are found for profiles from an individual line (e.g., [Fe vu] ^6087) taken from every object. In particular the relation between the velocity widths at \ and £ maximum intensity is the same found for the widths of the broad profiles of Hß in Seyfert 1 galaxies and QSOs by De Robertis (1984a). This may suggest that a similar acceleration mechanism (and/or geometry) operates in all objects in both the broad-and narrow-line regions. The high-ionization line widths correlate only poorly with the absolute blue magnitude of the galaxy, while the lower ionization lines show a good correlation. On average, half of the galaxies have narrow line profiles which are skewed to the blue, half which are symmetric. The low-ionization lines display little asymmetry in general, while the high-ionization lines tend to have blueward excesses. The possible implication of these and other correlations, and the absence of still other correlations, are discussed. Descriptions of the details of the individual spectra are presented. Subject headings: galaxies: Seyfert-line profiles 171

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Central black hole masses for 117 spiral galaxies representing morphological stages S0/a through Sc and taken from the large spectroscopic survey of Ho et al. are derived using K s -band data from the Two Micron All Sky Survey. Black hole masses are found using a calibrated black hole-K s bulge luminosity relation, while bulge luminosities are measured by means of a two-dimensional bulge-disk decomposition routine. The black hole masses are correlated against a variety of parameters representing properties of the nucleus and host galaxy. Nuclear properties such as line width (FWHM [N ii]), as well as emission-line ratios (e.g.,show a very high degree of correlation with black hole mass. The excellent correlation with line width supports the view that the emission-line gas is in virial equilibrium with either the black hole or bulge potential. The very good emission-line ratio correlations may indicate a change in ionizing continuum shape with black hole mass in the sense that more massive black holes generate harder spectra. Apart from the inclination-corrected rotational velocity, no excellent correlations are found between black hole mass and host galaxy properties. Significant differences are found between the distributions of black hole masses in early-, mid-, and late-type spiral galaxies (subsamples A, B, and C) in the sense that early-type galaxies have preferentially larger central black holes, consistent with observations that Seyfert galaxies are found preferentially in early-type systems. The line width distributions show a marked difference among subsamples A, B, and C in the sense that earlier type galaxies have larger line widths. There are also clear differences in line ratios between subsamples A+B and C that likely are related to the level of ionization in the gas. Finally, a K s -band Simien & de Vaucouleurs diagram shows excellent agreement with the original B-band relation, although there is a large dispersion at a given morphological stage.