Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

of the reduced spectrum for each slit position observed on each galaxy, along with
(ii) Gaussian line fits to the same (see §4.1).
3.3 Analysis
In this section we describe the line fitting that we carried out on each spectral row
of each reduced CCD spectral image, firstly with a single Gaussian per spectral line
(§4.1) and secondly with the inclusion of an additional free component (§4.2). In
§4.3 we discuss the sizes of the errors on quoted parameters from various sources. In
§4.4 we describe each of the UGC FR-I sample members in turn. For each galaxy
we define the central spectrum as the row with the greatest integrated flux after the
data reduction. We list the row numbers in the final x2d image corresponding to the
central spectrum in Table 3.1.
3.3.1 Single Gaussian line fitting
In the G750M spectra we expect to find the emission lines in the vicinity of Hα that are
listed in Table 3.4. We used wavelengths from the recent measurements of Wallerstein
et al. (2001) and converted from air to vacuum wavelengths using the IAU standard
formula
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