3 Results

The resulting stellar and ionized-gas kinematics of all our sample galaxies are shown in Fig. 2. Their relevant kinematic properties such as velocity gradients and velocity dispersions for both the stellar and gaseous components at different radii are given in Table A.1.

For each object the plot of the stellar and gaseous kinematics is organized as it follows:

1.

We display in the upper panel an image of the galaxy. We obtained the images for most of the sample galaxies in February and November 1997 at the 1.8-m Vatican Advanced Technology (VATT) in Arizona (USA), in December 1997 at the 0.8-m IAC80 telescope in Tenerife (Spain), and in March 1998 at the ESO 3.6-m telescope in La Silla (Chile). For the remaining galaxies we used an image taken either from the INT archive or the Digital Sky Survey (see Table 7). All images (except for the DSS ones) were bias-subtracted, flat-field corrected and cleaned for cosmic rays. The galaxy frames have been rotated and the slit position has been plotted to perform a better comparison between morphological and kinematic properties. The slit width and length correspond to those adopted in obtaining the spectra;

 

 

Table 7: Source of the images of sample galaxies.

Object	Source	Band
NGC 224	DSS
NGC 470	IAC80	$R_{\rm J}$
NGC 772	VATT	$R_{\rm C}$
NGC 949	VATT	$R_{\rm C}$
NGC 980	IAC80	$R_{\rm J}$
NGC 1160	VATT	$R_{\rm C}$
NGC 2541	IAC80	$R_{\rm J}$
NGC 2683	INT Archive	$R_{\rm C}$
NGC 2841	IAC80	$R_{\rm J}$
NGC 3031	DSS
NGC 3200	DSS
NGC 3368	INT Archive	$R_{\rm C}$
NGC 3705	DSS
NGC 3810	DSS
NGC 3898	VATT	$R_{\rm C}$
NGC 4419	VATT	$R_{\rm C}$
NGC 5064	ESO 3.6-m	$R_{\rm C}$
NGC 5854	IAC80	$R_{\rm J}$
NGC 7331	INT Archive	$R_{\rm C}$
NGC 7782	VATT	$R_{\rm C}$

2.

In the second panel we plot the velocity curves of the stellar (filled circles) and gaseous (open circles) components. The velocities are as observed without any inclination correction. Error bars are not plotted when smaller than symbols. The position angle of the slit is specified;

3.

In the third panel we plot in radial profiles the velocity dispersion of the stellar (filled circles) and gaseous (open circles) components. Error bars are not plotted when smaller than symbols;

4.

In the lower panels we plot the h₃ and h₄ radial profiles, respectively. h₃ and h₄ values are not given where the S/N ratio of the spectra was too low to allow a reliable measurement.

A detailed study of the ionized gas and stellar kinematics of NGC 772, NGC 3898 and NGC 7782 is given in Pignatelli et al. (2001). They combined kinematical data with V-band surface photometry in order to derive the mass distribution via a self-consistent Jeans model. Kinematic data for these galaxies are presented here for sake of completeness.

The kinematic parameters of the nearby galaxies NGC 224 and NGC 3031 have been measured by several authors. We decided to observe these galaxies to perform a consistency check of our measurements with the data available in the literature.

Figure 2: Stellar and ionized-gas kinematics of the sample galaxies. For NGC 470 some isophotes are traced to highlight the presence of the bar, whose major axis is drawn with a dashed line.

Figure 2: continued.

Figure 2: continued.

Figure 2: continued.

Figure 2: continued.

Figure 2: continued.

Figure 3: Velocity dispersion of stars and ionized gas measured in the centre ( upper panel) and at $R_{\rm e}/4$ ( lower panel) of the disc galaxies studied in this paper, Bertola et al. (1995); Fisher (1997) and Corsini et al. (1999). The different symbols refer to the different morphological types (as they appear in RC3). The continuous lines correspond to $\sigma _{\rm g}$$\;=\;$σ*. The ranges where $\sigma \le 60$  $\rm km\;s^{-1}$ are marked as a reference.