All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,clip]{H4111F1.eps}} \end{figure}$ Figure 1: Representative sample of continuum subtracted stellar templates used in this paper. The most important features found in those spectra have been indicated: the Paschen series (from P11 to P18), the Ca II triplet (Ca1, Ca2 and Ca3) and several metal lines (Fe I, Mg I and Ti I).
Open with DEXTER

In the text

$\begin{figure} \includegraphics[width=8.8cm,angle=0,clip]{H4111F2.eps} \end{figure}$ Figure 2: $\chi ^2$ distribution for NGC 5326. Open square indicates the minimum $\chi ^2$ for the best SSP fitting model, from which kinematics has been derived for this galaxy. $\chi ^2$ values for the stellar templates A2 Iab, F2 Ibe, G0 V and M4 Ve have been plotted with arrows indicating that they fall outside the plot limits. Their $\chi ^2$ values are: 2.197, 1.313, 0.613, 1.715 respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{H4111F3.eps} \end{figure}$ Figure 3: Comparison between our best stellar template, mix-template, and best SSP model fits, for the continuum subtracted and low-order filtered, binned central spectrum of NGC 5326. The fitting region has been indicated with a line at the bottom of the figure In this case the best fitting template is the SSP model.
Open with DEXTER

In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{H4111F4.eps}} \end{figure}$ Figure 4: Comparison of the profiles obtained with our best stellar templates (G8III, K2III, K3I, K3III, K5III, K6V, M1III), mix-template and best SSP model fit of NGC 5326.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4111F5.eps}} \end{figure}$ Figure 5: Recovery of $\sigma$ and h₄ via FOURFIT using SSP models and stellar templates. The left panels show the distribution of the recovered LOSVDs compared to the input ones at each sampled value of $\sigma$ and h₄ for each test at S/N>33. The right panels, on the other hand, show the total distribution (i.e. the sum of the individual ones on the right panels). For each $\sigma$ and h₄we plot a histogram of the $\Delta$ ( $\sigma )=\sigma ({\rm out})-\sigma$ (in) and $\Delta (h_4)=\rm h_4(out)-h_4(in)$ obtained from the 14 400 realisations corresponding to 8 white noise realizations. The values shown below each histogram represent the median (within square brackets) and standard deviation found at those values of $\sigma$ and h₄.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4111F6.eps} \end{figure}$ Figure 6: Comparison between our best SSP model fit and Vega Beltrán et al. (2001) for NGC 5854.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4111F7.eps} \end{figure}$ Figure 7: Comparison between our best SSP model fit with Fisher et al. (1994) (F94) and Simien & Prugniel (1997) (SP97) for NGC 7332.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,clip]{H4111F8.eps}} \end{figure}$ Figure 8: Velocity dispersion profiles for our sample of galaxies. Bulges with centrally-peaked velocity dispersions profiles are drawn in the top panel, whereas bulges with flat velocity dispersion profiles are plotted in the bottom panel. In the abscissa, radii have been normalized to the minor axis bulge radius (Table 1, Col. 12), defined as the radius along the minor axis where bulge and disk have equal surface brightness.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[clip]{H4111F9.eps}} \end{figure}$ Figure 9: Dependency of the velocity dispersion gradient on galaxy parameters. a) $\nabla \sigma$ against face-on H-band disk central surface brightness $\mu _{\rm0,D}$ . b) $\nabla \sigma$ against bulge ellipticity $\epsilon _{\rm B}$ . c) $\nabla \sigma$ against disk ellipticity $\epsilon _{\rm D}$ . Barred or box-peanut shaped galaxies in our sample are represented with open triangles.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[height=10.5cm,angle=0]{H4111_n5326.eps... ...}\hfill \includegraphics[height=10.5cm,angle=0]{H4111_n5443.eps} }\end{figure}$

In the text

$\begin{figure}\par\mbox{\includegraphics[height=10.5cm,angle=0]{H4111_n5475.eps}... ...}\hfill \includegraphics[height=10.5cm,angle=0]{H4111_n5707.eps} }\end{figure}$

In the text

$\begin{figure}\par\mbox{\includegraphics[height=10.5cm,angle=0]{H4111_n5719.eps}... ...}\hfill \includegraphics[height=10.5cm,angle=0]{H4111_n5854.eps} }\end{figure}$

In the text

$\begin{figure}\par\mbox{\includegraphics[height=10.5cm,angle=0]{H4111_n5879.eps}... ...}\hfill \includegraphics[height=10.5cm,angle=0]{H4111_n6504.eps} }\end{figure}$

In the text

$\begin{figure}\par\mbox{\includegraphics[height=10.5cm,angle=0]{H4111_n7331.eps}... ...ludegraphics[height=10.5cm,angle=0]{H4111_n7457.eps}\hspace*{4cm}}\end{figure}$

In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90,clip]{H4111F1.eps}} \end{figure}$	Figure 1: Representative sample of continuum subtracted stellar templates used in this paper. The most important features found in those spectra have been indicated: the Paschen series (from P11 to P18), the Ca II triplet (Ca1, Ca2 and Ca3) and several metal lines (Fe I, Mg I and Ti I).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=14cm,clip]{H4111F3.eps} \end{figure}$	Figure 3: Comparison between our best stellar template, mix-template, and best SSP model fits, for the continuum subtracted and low-order filtered, binned central spectrum of NGC 5326. The fitting region has been indicated with a line at the bottom of the figure In this case the best fitting template is the SSP model.
Open with DEXTER

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{H4111F4.eps}} \end{figure}$	Figure 4: Comparison of the profiles obtained with our best stellar templates (G8III, K2III, K3I, K3III, K5III, K6V, M1III), mix-template and best SSP model fit of NGC 5326.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4111F6.eps} \end{figure}$	Figure 6: Comparison between our best SSP model fit and Vega Beltrán et al. (2001) for NGC 5854.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4111F7.eps} \end{figure}$	Figure 7: Comparison between our best SSP model fit with Fisher et al. (1994) (F94) and Simien & Prugniel (1997) (SP97) for NGC 7332.
Open with DEXTER

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[clip]{H4111F9.eps}} \end{figure}$	Figure 9: Dependency of the velocity dispersion gradient on galaxy parameters. a) $\nabla \sigma$ against face-on H-band disk central surface brightness $\mu _{\rm0,D}$ . b) $\nabla \sigma$ against bulge ellipticity $\epsilon _{\rm B}$ . c) $\nabla \sigma$ against disk ellipticity $\epsilon _{\rm D}$ . Barred or box-peanut shaped galaxies in our sample are represented with open triangles.
Open with DEXTER