The line dispersion for an emission line $\sigma _{\rm line}$ should not be confused with the host galaxy bulge velocity disperion ${\sigma _*}$ .

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We have suppressed the point corresponding to the Wise Observatory data from 1988 which is not reliable on account of a variable line-spread function, as noted by Peterson et al. (2004).

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... mass

It is perhaps interesting that prior to the actual calibration of the reverberation-based mass scale by Onken et al. (2004), it was common to assume f=0.75 (Netzer 1990; Wandel et al. 1999; Kaspi et al. 2000) for FWHM-based mass estimates.

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... all

One Seyfert 2 galaxy, NGC 4258, whose BH mass was measured by megamaser motions (Miyoshi et al. 1995), was included in the sample of galaxies that defined the $M_{\rm BH}$ - ${\sigma _*}$ relationship.

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... considered

It is worthwhile recalling that when we speak of a "disk,'' it does not necessarily mean a continuous medium, but could refer to a clumpy medium made of an ensemble of clouds.

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... 14 objects

Note that for the sake of simplicity, we will restrict the discussion only to quantities derived from the mean spectra since these do not differ significantly from those derived from the rms spectra. Also, in the cases of sources for which multiple datasets are available, we use an average value of VP so that each source is counted only once.

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...1998)

In the course of these computations, we have confirmed that the analytical formulae for $R_{\rm sg}$ given by Kawaguchi et al. (2004a) show consistent results (with systematically larger values by a factor of $\sim$ 1.5).

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