All Figures

$\begin{figure} \par\includegraphics[width=4cm,clip]{3529f1a.ps}\hspace*{2mm} \in... ...9f1c.ps}\hspace*{2mm} \includegraphics[width=4cm,clip]{3529f1d.ps} \end{figure}$ Figure 1: Distribution of B-magnitudes ( first panel), morphological types ( second panel), heliocentric velocity ( third panel) and galaxy density ( forth panel).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3529f2.ps} \end{figure}$ Figure 2: Spectra of a representative galaxy in the sample. The figure shows the gradients obtained sampling each long-slit spectrum in four regions: between $0 \leq r \leq r_{\rm e}$ /16 (indicated as "nuclear'' in the figure), $r_{\rm e}/16 \leq r \leq r_{\rm e}$ /8, $r_{\rm e}/8 \leq r \leq r_{\rm e}$ /4 and $r_{\rm e}/4 \leq r \leq r_{\rm e}$ /2. For each region the figure overplots the two opposite sides of the galaxies with respect to the nucleus. With the exclusion of few cases (see text), the two sides agree within few percent. The major difference between the two sides often reside in the emission line distribution which is not symmetric with respect to the nucleus.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3529f3.ps} \end{figure}$ Figure 3: Comparison between central velocity dispersions used in this paper and in Trager et al. (1998). The lines indicate an average error (20 km s^-1) in the central velocity dispersion measurements.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3529f4a.ps}\hspace*{3mm} \includegraphics[width=7.1cm,clip]{3529f4b.ps} \end{figure}$ Figure 4: ( Left four panels) Comparison between the correction estimate of the $\rm H\beta$ emission derived from $\rm [OIII]$ emission line and from the H $\alpha$ emission (see Sect. 4.3). The solid line is the one-to-one relation assuming for O[III] valid the formula $EW({\rm H}\beta _{\rm em})/EW\rm ([OIII]\lambda 5007) = 0.7$ . The comparison is shown in the four regions sampled by the linear gradients (legend: lg1 ( $0 \leq r \leq r_{\rm e}$ /16 ("nuclear'')), lg2 ( $r_{\rm e}/16 \leq r \leq r_{\rm e}$ /8), lg3 ( $r_{\rm e}/8 \leq r \leq r_{\rm e}$ /4) and lg4 ( $r_{\rm e}/4 \leq r \leq r_{\rm e}$ /2). Open circles indicate galaxies which O[III] emission is detected under 1 $\sigma$ level, triangles and full squares between 1 and 2 $\sigma$ levels and above 2 $\sigma$ level respectively (see text). ( Right four panels) Fitting of N[II]( $\lambda$ 6548, 6584) and H $\alpha$ lines for two representative galaxies: one with H $\alpha$ in emission (NGC 2749) and the second with the H $\alpha$ infilling (IC 2006). Lower panels show the residuals lines after the subtraction of the H $\alpha$ line of the template galaxy NGC 1426 (dotted lines in the upper panels).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14.8cm,clip]{3529f5.ps} \end{figure}$ Figure 5: Comparison of passband measurements from our spectra and original Lick data for 17 Lick standard stars. The dotted line is the one to one relation while the solid line is the robust straight-line fit to the filled squares.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.4cm,clip]{3529f6.ps} \end{figure}$ Figure 6: Comparison of index measurements of González (1993: open triangles), Trager (1998: full squares), Longhetti et al. (1998: open circles), Beuing et al. (2002: open pentagons) with our data. Solid lines mark the one-to-one relation. Table 11 summarizes the results of the comparison.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3529f7.ps} \end{figure}$ Figure 7: Mg₂ versus $\sigma$ relation. Our Mg₂ line-strength indices measured within the SLOAN aperture (r=1.5 $^{\prime \prime }$ ) are plotted after the transformation to the Lick-IDS system. The solid dashed line is the least-square fit obtained Trager et al. (1998). The the dotted and long-dashed lines represent the least-square fit obtained by Bernardi et al. (1998) for the field sample of 631 galaxies and our fit (value at $\sigma_{300~\rm km~s^{-1}} = 0.339$ , slope of relation = 0.214) to the present data respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f8.ps} \end{figure}$ Figure 8: Fully corrected Mg₂ line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f9.ps} \end{figure}$ Figure 9: As in Fig. 8.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f10.ps} \end{figure}$ Figure 10: Fully corrected H $\beta$ line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f11.ps} \end{figure}$ Figure 11: As in Fig. 10.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f12.ps} \end{figure}$ Figure 12: Fully corrected Fe5335 line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f13.ps} \end{figure}$ Figure 13: As in Fig. 12.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{3529f1a.ps}\hspace{2mm} \in... ...9f1c.ps}\hspace{2mm} \includegraphics[width=4cm,clip]{3529f1d.ps} \end{figure}$	Figure 1: Distribution of B-magnitudes ( first panel), morphological types ( second panel), heliocentric velocity ( third panel) and galaxy density ( forth panel).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3529f3.ps} \end{figure}$	Figure 3: Comparison between central velocity dispersions used in this paper and in Trager et al. (1998). The lines indicate an average error (20 km s^-1) in the central velocity dispersion measurements.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=14.8cm,clip]{3529f5.ps} \end{figure}$	Figure 5: Comparison of passband measurements from our spectra and original Lick data for 17 Lick standard stars. The dotted line is the one to one relation while the solid line is the robust straight-line fit to the filled squares.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=15.4cm,clip]{3529f6.ps} \end{figure}$	Figure 6: Comparison of index measurements of González (1993: open triangles), Trager (1998: full squares), Longhetti et al. (1998: open circles), Beuing et al. (2002: open pentagons) with our data. Solid lines mark the one-to-one relation. Table 11 summarizes the results of the comparison.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f8.ps} \end{figure}$	Figure 8: Fully corrected Mg₂ line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f9.ps} \end{figure}$	Figure 9: As in Fig. 8.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f10.ps} \end{figure}$	Figure 10: Fully corrected H $\beta$ line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f11.ps} \end{figure}$	Figure 11: As in Fig. 10.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f12.ps} \end{figure}$	Figure 12: Fully corrected Fe5335 line-strength index as function of the luminosity weighted radius normalized to the galaxy equivalent radius $R_{\rm e}$ . Apertures are indicated with open squares, while gradients are indicated with full dots.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{3529f13.ps} \end{figure}$	Figure 13: As in Fig. 12.
Open with DEXTER