All Figures

$\begin{figure} \par\includegraphics[width=8cm]{6578f1.ps} \end{figure}$ Figure 1: The photometric error, as determined by ALLSTAR, for a CCD which includes IC 1613. To reduce the colour scatter we exclude objects with magnitude error, both in i' and g', less than 0.15.
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In the text

$\begin{figure} \par\includegraphics[width=5cm]{6578f2.ps} \end{figure}$ Figure 2: Distributions of the SHARP parameter for objects with photometric error <0.15 mag. The upper panel corresponds to two CCDs within IC 1613 while the bottom panel is for two CCDs outside the galaxy. We see a huge population of non-stellar objects brighter that the magnitude limit. Close to the magnitude limit, SHARP becomes meaningless due to the large scatter. The dashed line marks the saturation threshold.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6578f3.ps}\par\end{figure}$ Figure 3: Spatial distribution of all stars with i'< 24.0 and selected following the SHARP criterion described above.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6578f4.ps} \end{figure}$ Figure 4: Colour-magnitude diagram of the whole field, 63 000 objects satisfying the error and SHARP criteria, are plotted. The giant box encloses the RGB and AGB stars, while the blue stars are in the left region. The white line marks the 75% completeness level for the RGB stars that will be used for the structural study of the galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6578f5.ps} \end{figure}$ Figure 5: Same as Fig. 4 but for objects rejected because of their high SHARP.
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In the text

$\begin{figure} \par\includegraphics[width=5cm]{6578f6.ps} \end{figure}$ Figure 6: Spatial distributions of the blue main sequence stars ( top panel) and RGB + AGB stars ( lower panel). Representative HI isodensity contours, from Hoffman et al. (1996) are traced. Each panel corresponds to one square degree of the sky. Big white dots indicate the position of the center calculated for the RGB+AGB sample.
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In the text

$\begin{figure} \par\includegraphics[width=5cm]{6578f7.ps} \end{figure}$ Figure 7: Solutions for the position angles and ellipticities for elliptical isodensity contours.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm]{6578f8.ps} \end{figure}$ Figure 8: The observed density profile of the giants. A close up of the tail is shown in the small panel.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{6578f9.ps} \end{figure}$ Figure 9: The corrected surface density profile of the spheroid, defined by its giants, is not exponential.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{6578f10.ps} \end{figure}$ Figure 10: A King model is fitted to the surface density of giants in the spheroid. Dashed line is an extrapolation of the fit. Error bars are omitted to better show the dispersion of the points along the curve.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{6578f11.ps} \end{figure}$ Figure 11: A Sérsic law fitted to the observed profile for r>5'. Dashed line is an extrapolation of the fit.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{6578f1.ps} \end{figure}$	Figure 1: The photometric error, as determined by ALLSTAR, for a CCD which includes IC 1613. To reduce the colour scatter we exclude objects with magnitude error, both in i' and g', less than 0.15.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm]{6578f3.ps}\par\end{figure}$	Figure 3: Spatial distribution of all stars with i'< 24.0 and selected following the SHARP criterion described above.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm]{6578f4.ps} \end{figure}$	Figure 4: Colour-magnitude diagram of the whole field, 63 000 objects satisfying the error and SHARP criteria, are plotted. The giant box encloses the RGB and AGB stars, while the blue stars are in the left region. The white line marks the 75% completeness level for the RGB stars that will be used for the structural study of the galaxy.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm]{6578f5.ps} \end{figure}$	Figure 5: Same as Fig. 4 but for objects rejected because of their high SHARP.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm]{6578f6.ps} \end{figure}$	Figure 6: Spatial distributions of the blue main sequence stars ( top panel) and RGB + AGB stars ( lower panel). Representative HI isodensity contours, from Hoffman et al. (1996) are traced. Each panel corresponds to one square degree of the sky. Big white dots indicate the position of the center calculated for the RGB+AGB sample.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm]{6578f7.ps} \end{figure}$	Figure 7: Solutions for the position angles and ellipticities for elliptical isodensity contours.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm]{6578f8.ps} \end{figure}$	Figure 8: The observed density profile of the giants. A close up of the tail is shown in the small panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm]{6578f9.ps} \end{figure}$	Figure 9: The corrected surface density profile of the spheroid, defined by its giants, is not exponential.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm]{6578f10.ps} \end{figure}$	Figure 10: A King model is fitted to the surface density of giants in the spheroid. Dashed line is an extrapolation of the fit. Error bars are omitted to better show the dispersion of the points along the curve.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm]{6578f11.ps} \end{figure}$	Figure 11: A Sérsic law fitted to the observed profile for r>5'. Dashed line is an extrapolation of the fit.
Open with DEXTER