All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{8232f1.eps}} \end{figure}$ Figure 1: The V-band Suprime-Cam image of Ursa Major I dSph covering a field of 34 $^\prime$ $\times$ 27 $^\prime$ . North is to the top and east is to the left.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90]{8232f2.eps}} \end{figure}$ Figure 2: Completeness of I (solid line) and V (doted line) photometry. The horizontal dotted line represents the 90 $\%$ level.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{ \includegraphics{8232f3a.eps} \includegraphics{8232f3b.eps} } \end{figure}$ Figure 3: Colour-magnitude diagrams of the UMa I dSph. Error bars show the photometric error at each magnitude level based on the artificial star test. The boundaries marked in the top-left panel are used to select stars belonging to the main sequence, giant branch and horizontal branch and blue strugglers of the UMa I dSph.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{ \includegraphics{8232f4a.eps} \includegraphics{8232f4b.eps} } \end{figure}$ Figure 4: Left: V-band colour-magnitude diagram of the UMa I dSph with the fiducial sequence of Galactic globular clusters (M 3, M 5, M 92). Right: the theoretical isochrones overlaid in the V-band colour-magnitude diagram of the UMa I dSph. The lines stand for the interpolated Padova isochrones for $\rm [Fe/H]=-2.0$ and ages of 10.0, 12.6, 14.1 Gyr which were shifted according to the distance of the UMa I dSph.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{8232f5.eps}} \end{figure}$ Figure 5: Upper: the spatial distribution of the stars selected by the dashed lines in Fig. 3, which cover the central 730 pc $\times$ 670 pc of the UMa I dSph. Lower: the isodensity contour of the CMD-selected sources. The plotted contour levels are 1-10 $\sigma$ above the background level.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90]{8232f6.eps}} \end{figure}$ Figure 6: Radial profile derived by calculating the average number density within elliptical annuli. The effect of foreground stars is corrected by using a Galactic model (Girardi et al. 2005). The best-fitting exponential profile with the effective radius $r_{\rm e}=6.73\hbox {$^\prime $ }\pm 0.30\hbox {$^\prime $ }$ and Plummer profile with the Plummer radius $b=10.42\hbox {$^\prime $ }\pm 0.76\hbox {$^\prime $ }$ have been overlaid as the dashed line and dotted line, respectively.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{8232f1.eps}} \end{figure}$	Figure 1: The V-band Suprime-Cam image of Ursa Major I dSph covering a field of 34 $^\prime$ $\times$ 27 $^\prime$ . North is to the top and east is to the left.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90]{8232f2.eps}} \end{figure}$	Figure 2: Completeness of I (solid line) and V (doted line) photometry. The horizontal dotted line represents the 90 $\%$ level.
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$\begin{figure} \par\resizebox{18cm}{!}{ \includegraphics{8232f3a.eps} \includegraphics{8232f3b.eps} } \end{figure}$	Figure 3: Colour-magnitude diagrams of the UMa I dSph. Error bars show the photometric error at each magnitude level based on the artificial star test. The boundaries marked in the top-left panel are used to select stars belonging to the main sequence, giant branch and horizontal branch and blue strugglers of the UMa I dSph.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{8232f5.eps}} \end{figure}$	Figure 5: Upper: the spatial distribution of the stars selected by the dashed lines in Fig. 3, which cover the central 730 pc $\times$ 670 pc of the UMa I dSph. Lower: the isodensity contour of the CMD-selected sources. The plotted contour levels are 1-10 $\sigma$ above the background level.
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