All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig1.ps}\end{figure}$ Figure 1: The stellar kinematical measurements along the major axis of NGC 1052. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Binney et al. (1990), open squares, and Fried & Illingworth (1994), open triangles, are presented as well.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig2.ps}\end{figure}$ Figure 2: The stellar kinematical measurements along the minor axis of NGC 1052. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Binney et al. (1990), open squares, are presented as well.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig3.ps}\end{figure}$ Figure 3: The stellar kinematical measurements along the major axis of NGC 7796. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Bertin et al. (1994), open squares, are presented as well.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig4.ps}\end{figure}$ Figure 4: The stellar kinematical measurements along the minor axis of NGC 7796. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig5.ps}\end{figure}$ Figure 5: Radial gradients of Fe4383, Fe4531, Fe4668, Fe5270, Fe5335 and $\langle {\rm Fe}\rangle$ along both axes of NGC 1052 whose respective linear regressions are shown by solid and dashed lines for the major (solid squares) and minor axis (solid circles) data respectively. The seeing size $\sigma _{\rm seeing}$ is given on the abscissa of the bottom-left plot ( $\sigma _{\rm seeing} = {\it FWHM}_{\rm seeing}$ /2.355). The Fe5270 data of Carollo et al. (1993) along the E-W direction, open triangles, are also plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig6.ps}\end{figure}$ Figure 6: Radial gradients of Fe5406, Fe5709, Fe5782, Ca4455, Mg b and Na D along both axes of NGC 1052. The notation is the same as in Fig. 5. The Na D data of Carollo et al. (1993) along the E-W direction, open triangles, are also plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{4615fig7.ps}\end{figure}$ Figure 7: Radial gradients of Mg₁ and Mg₂along both axes of NGC 1052. The notation is the same as in Fig. 5. The fit for the minor axis Mg₂ data is not plotted. The Mg₂ data of Couture & Hardy (1988) along the major and minor axis, open squares and open triangles respectively, are also plotted ( bottom panel). The Mg₁ and Mg₂ data of Carollo et al. (1993) along the E-W direction, open pentagons, are plotted ( both panels).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig8.ps}\end{figure}$ Figure 8: Radial gradients of Fe4383, Fe4531, Fe4668, Fe5270, Fe5335 and $\langle {\rm Fe}\rangle$ along both axes of NGC 7796. The notation is the same as in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig9.ps}\end{figure}$ Figure 9: Radial gradients of Fe5406, Fe5709, Fe5782, Ca4455, Mg b and Na D along both axes of NGC 7796. The notation is the same as in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg10.ps}\end{figure}$ Figure 10: Radial gradients of H $\beta$ , Mg₁ and Mg₂ along both axes of NGC 7796. The notation is the same as in Fig. 5. The Mg₂ data of Bertin et al. (1994) along the major, open squares, are also plotted ( bottom panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg11.ps}\end{figure}$ Figure 11: a) Mg b versus Fe4531 plot ( top panel); b) Mg b versus Fe5270 plot ( bottom panel): comparisons of Lick indices of the long slit spectra of NGC 1052 (both photometric axes) with the theoretical ones of TMB (2003a)'s SSPs. The index values of the spectra are represented by solid black squares for the major axis data and solid black circles for the minor axis data, which are both connected by traced black lines. The index errors are only plotted for the central spectrum data. The SSP predicted index values are represented by open symbols whose colour indicate the curve families with different [ $\alpha$ /Fe]: -0.3 (blue), 0.0 (green), +0.3 (yellow) and +0.5 dex (red). The SSP ages are represented by open symbols: 2 (crosses), 6 (four-points stars), 10 (triangles), 12 (squares) and 15 Gyr (pentagons). The global metallicities, [ $Z/Z_{\odot }] = -2.2$ 5, -1.35, -0.33, 0.00, +0.35, +0.67 dex, increase from the left-bottom to the right-top for a given [ $\alpha$ /Fe] family curve. The predicted Lick indices of the SSPs with 10 Gyr and different [ $\alpha$ /Fe] are connected by solid black lines for a specific metallicity.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg12.ps}\end{figure}$ Figure 12: a) Mg b versus Fe5335; Mg b versus Fe5406 b): comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg13.ps}\end{figure}$ Figure 13: a) Mg b versus Fe5709; b) Mg b versus Fe5782: comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg14.ps}\end{figure}$ Figure 14: a) Mg₁ versus $\langle {\rm Fe}\rangle$ ; b) Mg₂ versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg15.ps}\end{figure}$ Figure 15: Na D versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg16.ps}\end{figure}$ Figure 16: [MgFe] $_{\rm TMB}$ modified Lick index versus H $\beta$ Lick index: comparison of Lick indices of the long slit spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The indices of the aperture spectra are represented by solid black squares (major axis data for $6.8 \leq r \leq 20.2$ arcsec) and solid black circles (minor axis data for $6.8\leq r \leq 18.0$ arcsec) which are connected by traced black lines as in Fig. 15. The predicted indices of the SSPs are represented by open colour symbols (ages by symbols and [ $\alpha$ /Fe] by colours), however the solid black lines connect the Lick indices of the SSPs with [ $\alpha$ /Fe] = 0.0 dex for each global metallicity covering different ages. In this plot, the global metallicities increase from the bottom to the top.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4615fg17.ps}\end{figure}$ Figure 17: a) Mg b versus Fe4531; b) Mg b versus Fe5270: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4615fg18.ps}\end{figure}$ Figure 18: a) Mg b versus Fe5335; b) Mg b versus Fe5406: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg19.ps}\end{figure}$ Figure 19: a) Mg b versus Fe5709; b) Mg b versus Fe5782: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg20.ps}\end{figure}$ Figure 20: a) Mg₁ versus $\langle {\rm Fe}\rangle$ ; b) Mg₂ versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg21.ps}\end{figure}$ Figure 21: Na D versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg22.ps}\end{figure}$ Figure 22: [MgFe] $_{\rm TMB}$ versus H $\beta$ : comparison of Lick indices of the long slit spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 16. In this plot, the global metallicities increase from the bottom to the top.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg23.ps}\end{figure}$ Figure 23: Spectra of the stellar population templates used in the synthesis, normalized to $\lambda 5870$ Å.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615f24a.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4615f24b.ps}\end{figure}$ Figure 24: Synthesis results of NGC 1052 in flux fractions as a function of the distance to the center along both photometric axes - panels a), b), c), d), e), f) and g) for the G1, G2, G3, Y1, Y2, Y3 and RHII components respectively; panel h) - spatial distribution of the internal reddening. Note that the abscissa axis has a different scale for each plot.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615f25a.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4615f25b.ps}\end{figure}$ Figure 25: Synthesis results of NGC 7796 in flux fractions as a function of the distance to the center along both photometric axes - panels a), b), c), d), e), f) and g) for each base component; panel h) - spatial distribution of the internal reddening (like Fig. 24).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615fg26.ps}\end{figure}$ Figure 26: Stellar population synthesis of the central extraction of NGC 1052 (major axis extraction). a) Observed spectrum corrected for reddening and template spectrum. b) Residual spectrum as an emission spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615fg27.ps}\end{figure}$ Figure 27: Stellar population synthesis of the central extraction of NGC 7796 (major axis extraction). a) Observed spectrum corrected for reddening and template spectrum. b) Residual spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig1.ps}\end{figure}$	Figure 1: The stellar kinematical measurements along the major axis of NGC 1052. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Binney et al. (1990), open squares, and Fried & Illingworth (1994), open triangles, are presented as well.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig2.ps}\end{figure}$	Figure 2: The stellar kinematical measurements along the minor axis of NGC 1052. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Binney et al. (1990), open squares, are presented as well.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig3.ps}\end{figure}$	Figure 3: The stellar kinematical measurements along the major axis of NGC 7796. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile. Our data are plotted using solid squares. The data of Bertin et al. (1994), open squares, are presented as well.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig4.ps}\end{figure}$	Figure 4: The stellar kinematical measurements along the minor axis of NGC 7796. a) The line-of-sight velocity rotation curve; b) the line-of-sight velocity dispersion radial profile.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig6.ps}\end{figure}$	Figure 6: Radial gradients of Fe5406, Fe5709, Fe5782, Ca4455, Mg b and Na D along both axes of NGC 1052. The notation is the same as in Fig. 5. The Na D data of Carollo et al. (1993) along the E-W direction, open triangles, are also plotted.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig8.ps}\end{figure}$	Figure 8: Radial gradients of Fe4383, Fe4531, Fe4668, Fe5270, Fe5335 and $\langle {\rm Fe}\rangle$ along both axes of NGC 7796. The notation is the same as in Fig. 5.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fig9.ps}\end{figure}$	Figure 9: Radial gradients of Fe5406, Fe5709, Fe5782, Ca4455, Mg b and Na D along both axes of NGC 7796. The notation is the same as in Fig. 5.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg10.ps}\end{figure}$	Figure 10: Radial gradients of H $\beta$ , Mg₁ and Mg₂ along both axes of NGC 7796. The notation is the same as in Fig. 5. The Mg₂ data of Bertin et al. (1994) along the major, open squares, are also plotted ( bottom panel).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg12.ps}\end{figure}$	Figure 12: a) Mg b versus Fe5335; Mg b versus Fe5406 b): comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg13.ps}\end{figure}$	Figure 13: a) Mg b versus Fe5709; b) Mg b versus Fe5782: comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg14.ps}\end{figure}$	Figure 14: a) Mg₁ versus $\langle {\rm Fe}\rangle$ ; b) Mg₂ versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg15.ps}\end{figure}$	Figure 15: Na D versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 1052 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4615fg17.ps}\end{figure}$	Figure 17: a) Mg b versus Fe4531; b) Mg b versus Fe5270: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4615fg18.ps}\end{figure}$	Figure 18: a) Mg b versus Fe5335; b) Mg b versus Fe5406: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg19.ps}\end{figure}$	Figure 19: a) Mg b versus Fe5709; b) Mg b versus Fe5782: comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg20.ps}\end{figure}$	Figure 20: a) Mg₁ versus $\langle {\rm Fe}\rangle$ ; b) Mg₂ versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg21.ps}\end{figure}$	Figure 21: Na D versus $\langle {\rm Fe}\rangle$ : comparisons of the observed Lick indices of the aperture spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 11.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4615fg22.ps}\end{figure}$	Figure 22: [MgFe] $_{\rm TMB}$ versus H $\beta$ : comparison of Lick indices of the long slit spectra of NGC 7796 with the theoretical ones of TMB (2003a)'s SSPs. The notation is the same as in Fig. 16. In this plot, the global metallicities increase from the bottom to the top.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4615fg23.ps}\end{figure}$	Figure 23: Spectra of the stellar population templates used in the synthesis, normalized to $\lambda 5870$ Å.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615f24a.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4615f24b.ps}\end{figure}$	Figure 24: Synthesis results of NGC 1052 in flux fractions as a function of the distance to the center along both photometric axes - panels a), b), c), d), e), f) and g) for the G1, G2, G3, Y1, Y2, Y3 and RHII components respectively; panel h) - spatial distribution of the internal reddening. Note that the abscissa axis has a different scale for each plot.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615f25a.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4615f25b.ps}\end{figure}$	Figure 25: Synthesis results of NGC 7796 in flux fractions as a function of the distance to the center along both photometric axes - panels a), b), c), d), e), f) and g) for each base component; panel h) - spatial distribution of the internal reddening (like Fig. 24).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615fg26.ps}\end{figure}$	Figure 26: Stellar population synthesis of the central extraction of NGC 1052 (major axis extraction). a) Observed spectrum corrected for reddening and template spectrum. b) Residual spectrum as an emission spectrum.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4615fg27.ps}\end{figure}$	Figure 27: Stellar population synthesis of the central extraction of NGC 7796 (major axis extraction). a) Observed spectrum corrected for reddening and template spectrum. b) Residual spectrum.
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