All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{8899fig1.ps}\end{figure}$ Figure 1: Location of globular clusters in M 31. Dark purple triangle corresponds to the location of G78, light blue circle corresponds to G213 and dark red square shows the location of G280. Numbered squared regions correspond to charts in the Atlas of the Andromeda Galaxy (Hodge 1981).
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{8899fig2.eps}\end{figure}$ Figure 2: MultiDrizzled images of G78 ( left), G213 ( middle) and G280 ( right) and surrounding field stars in the F814W filter. North is to the top, East is to the left. The dark feature seen on the northeast corresponds to the occulting finger of the ACS. Field of view (FoV) for each cluster is 17.3 $\hbox {$^{\prime \prime }$ }\times 17.3 \hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip]{8899fig3.ps}\end{figure}$ Figure 3: DAOPHOT/ALLSTAR output for G78. Top: error vs. magnitude for both F606W and F814W instrumental magnitudes. Middle: $\chi ^2$ vs. magnitude. Bottom: sharpness vs. magnitude. Solid lines show the upper limits for stars used to build the CMDs of the cluster and the field; dashed line shows the averaged value after iteration. In the case of the sharpness a lower limit was also used to select stars.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{8899fg6a.ps}\par\v... ...vspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{8899fg6c.ps}\end{figure}$ Figure 6: Left panels: color-magnitude diagrams (CMD) for G78 ( top), G213 ( middle) and G280 ( bottom) considering all stars within $R_{\rm out}$ - values given in Table 3. Right panels: CMDs considering all the stars in the field of view (FoV) of the MultiDrizzled HST-ACS images of G78 ( top), G213 ( middle) and G280 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.8cm,clip]{8899fg7a.ps}\par... ...ace*{2mm} \includegraphics[angle=270,width=6.8cm,clip]{8899fg7c.ps} \end{figure}$ Figure 7: Density profile for all stars in the FoV of G78 ( top), G213 ( middle) and G280 ( bottom) after statistical selection (see Sect. 4). Dashed lines delimit the region used to construct the CMD of each cluster. Dot-dashed lines delimit the region of the FoV used for the CMD of the surrounding stars (see Sect. 7.2). Apparent density holes near the center of the clusters are due to star crowding.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=4cm,clip]{8899fg8a.ps}\hspac... ...ncludegraphics[angle=270,width=4cm,clip]{8899fg8c.ps}\hspace*{2cm}} \end{figure}$ Figure 8: Results of the artificial stars experiments with no statistical selection of stars for G78 ( top left), G213 ( top right) and G280 ( bottom). The thin white solid line indicates the input RGB while the dots indicate the output (measured) RGB stars.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.3cm,clip]{8899fg9a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=6.3cm,clip]{8899fg9c.ps}\end{figure}$ Figure 9: Input and recovered magnitude difference according to radial position for G78 ( top), G213 ( middle) and G280 ( bottom). For each cluster, the inner lines correspond to 5.1 $\hbox {$^{\prime \prime }$ }$ , 3.7 $\hbox {$^{\prime \prime }$ }$ and 4.2 $\hbox {$^{\prime \prime }$ }$ for G78, G213 and G280, respectively, while the outer lines correpond to 6.4 $\hbox {$^{\prime \prime }$ }$ , 5.3 $\hbox {$^{\prime \prime }$ }$ and 5.6 $\hbox {$^{\prime \prime }$ }$ for G78, G213 and G280, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=4.8cm,clip]{8899f10a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=4.8cm,clip]{8899f10c.ps}\end{figure}$ Figure 10: Luminosity function (LF) for G78 ( top), G213 ( middle) and G280 ( bottom) and their corresponding surrounding fields. For each cluster, the LF was derived considering the following inner radii, $R_{\rm in}=5.1\hbox {$^{\prime \prime }$ }$ , 3.7 $\hbox {$^{\prime \prime }$ }$ , 4.2 $\hbox {$^{\prime \prime }$ }$ for G78, G213 and G280 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=4.8cm,clip]{8899f11a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=4.8cm,clip]{8899f11c.ps}\end{figure}$ Figure 11: Luminosity function (LF) for G78 ( top), G213 ( middle) and G280 ( bottom) subtracted from the contribution of their corresponding surrounding fields.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{8899f12a.ps}\par\v... ...vspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{8899f12c.ps}\end{figure}$ Figure 12: Superposition of the ridges and HB loci derived by Brown et al. (2005) on the CMD of G78 ( top), G213 ( middle) and G280 ( bottom). Thick solid line indicates the position of the fiducial RGB of each cluster. The straight dotted line shows the position of the red clump of each cluster.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{8899f13a.ps}\par\v... ...vspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{8899f13c.ps}\end{figure}$ Figure 13: Color-magnitude diagrams (CMD) for G78 ( top left), G213 ( middle left) and G280 ( bottom left) and corresponding surrounding fields, top right for G78, middle right for G213 and bottom right for G280. Grey dots indicate the stars considered for the fit of the RGB. Solid lines show the locus of this fiducial RGB. Black dots indicate the stars considered for computation of the RGB width. Right panels show the CMD for each surrounding region. Dark dots indicate stars considered for the analysis of the contribution of field stars to the width of the RGB of the cluster.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.2cm,clip]{8899f14a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=6.2cm,clip]{8899f14c.ps}\end{figure}$ Figure 14: Color histograms for each cluster, G78 ( top), G213 ( middle) and G280 ( bottom), and its corresponding surrounding fields. Solid straight lines show the simple histogram of both the cluster and the surrounding field derived by simple bining of stars per color interval. Dots (for the cluster) and crosses (for the surrounding field stars) display the histograms obtained by weighting the contribution of each star to each color bin with its associated photometric error. Solid lines indicate the Gaussian fit for each case.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=4cm,clip]{8899f15a.ps}\hspac... ...ncludegraphics[angle=270,width=4cm,clip]{8899f15c.ps}\hspace*{2cm}} \end{figure}$ Figure 15: Results of the artificial star experiments after applying the statistical selection of stars described in section 4 for G78 ( top left), G213 ( top right) and G280 ( bottom). The solid line indicates the input RGB while the dots indicate the output (measured) RGB stars. Only stars falling within each cluster annulus were considered.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{8899f16a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=7.2cm,clip]{8899f16c.ps}\end{figure}$ Figure 16: Resulting color histogram for G78 ( top), G213 ( middle) and G280 ( bottom). Filled dots display the color distribution of observed stars. Empty circles display the color distribution of recovered artificial stars. Solid and dashed lines showed the fitted Gaussians for each case.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=4.5cm,clip]{8899f17a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=4.5cm,clip]{8899f17c.ps}\end{figure}$ Figure 17: Color versus metallicity plot for a magnitude value of ${\it F814W}=0.435$ derived from the Brown et al. (2005) ridgelines. Solid line shows the fit of second order polynomial given by Eq. (1). Empty circle shows the position of the RGB of G78 at that magnitude value considering E(B-V)= 0.22 ( top left panel); empty circle shows the position of the RGB of G213 at that magnitude value considering a reddening of 0.1 ( top right panel); empty circle shows the position of the RGB of G280 at that magnitude value considering a reddening of 0.1 ( bottom panel). For all three panels, crosses indicate the lower and upper limits in color and metallicity used to determine the metallicity dispersion of each cluster.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip]{8899fig4.ps}\end{figure}$ Figure 4: DAOPHOT/ALLSTAR output for G213. Same as Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip]{8899fig5.ps}\end{figure}$ Figure 5: DAOPHOT/ALLSTAR output for G280. Same as Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8899fig1.ps}\end{figure}$	Figure 1: Location of globular clusters in M 31. Dark purple triangle corresponds to the location of G78, light blue circle corresponds to G213 and dark red square shows the location of G280. Numbered squared regions correspond to charts in the Atlas of the Andromeda Galaxy (Hodge 1981).
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$\begin{figure} \par\includegraphics[width=13cm,clip]{8899fig2.eps}\end{figure}$	Figure 2: MultiDrizzled images of G78 ( left), G213 ( middle) and G280 ( right) and surrounding field stars in the F814W filter. North is to the top, East is to the left. The dark feature seen on the northeast corresponds to the occulting finger of the ACS. Field of view (FoV) for each cluster is 17.3 $\hbox {$^{\prime \prime }$ }\times 17.3 \hbox {$^{\prime \prime }$ }$ .
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{8899fg6a.ps}\par\v... ...vspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{8899fg6c.ps}\end{figure}$	Figure 6: Left panels: color-magnitude diagrams (CMD) for G78 ( top), G213 ( middle) and G280 ( bottom) considering all stars within $R_{\rm out}$ - values given in Table 3. Right panels: CMDs considering all the stars in the field of view (FoV) of the MultiDrizzled HST-ACS images of G78 ( top), G213 ( middle) and G280 ( bottom).
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$\begin{figure} \par\includegraphics[angle=270,width=4cm,clip]{8899fg8a.ps}\hspac... ...ncludegraphics[angle=270,width=4cm,clip]{8899fg8c.ps}\hspace*{2cm}} \end{figure}$	Figure 8: Results of the artificial stars experiments with no statistical selection of stars for G78 ( top left), G213 ( top right) and G280 ( bottom). The thin white solid line indicates the input RGB while the dots indicate the output (measured) RGB stars.
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$\begin{figure} \par\includegraphics[angle=270,width=4.8cm,clip]{8899f10a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=4.8cm,clip]{8899f10c.ps}\end{figure}$	Figure 10: Luminosity function (LF) for G78 ( top), G213 ( middle) and G280 ( bottom) and their corresponding surrounding fields. For each cluster, the LF was derived considering the following inner radii, $R_{\rm in}=5.1\hbox {$^{\prime \prime }$ }$ , 3.7 $\hbox {$^{\prime \prime }$ }$ , 4.2 $\hbox {$^{\prime \prime }$ }$ for G78, G213 and G280 respectively.
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$\begin{figure} \par\includegraphics[angle=270,width=4.8cm,clip]{8899f11a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=4.8cm,clip]{8899f11c.ps}\end{figure}$	Figure 11: Luminosity function (LF) for G78 ( top), G213 ( middle) and G280 ( bottom) subtracted from the contribution of their corresponding surrounding fields.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{8899f12a.ps}\par\v... ...vspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{8899f12c.ps}\end{figure}$	Figure 12: Superposition of the ridges and HB loci derived by Brown et al. (2005) on the CMD of G78 ( top), G213 ( middle) and G280 ( bottom). Thick solid line indicates the position of the fiducial RGB of each cluster. The straight dotted line shows the position of the red clump of each cluster.
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$\begin{figure} \par\includegraphics[angle=270,width=4cm,clip]{8899f15a.ps}\hspac... ...ncludegraphics[angle=270,width=4cm,clip]{8899f15c.ps}\hspace*{2cm}} \end{figure}$	Figure 15: Results of the artificial star experiments after applying the statistical selection of stars described in section 4 for G78 ( top left), G213 ( top right) and G280 ( bottom). The solid line indicates the input RGB while the dots indicate the output (measured) RGB stars. Only stars falling within each cluster annulus were considered.
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$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{8899f16a.ps}\par... ...pace*{2mm} \includegraphics[angle=270,width=7.2cm,clip]{8899f16c.ps}\end{figure}$	Figure 16: Resulting color histogram for G78 ( top), G213 ( middle) and G280 ( bottom). Filled dots display the color distribution of observed stars. Empty circles display the color distribution of recovered artificial stars. Solid and dashed lines showed the fitted Gaussians for each case.
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$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip]{8899fig4.ps}\end{figure}$	Figure 4: DAOPHOT/ALLSTAR output for G213. Same as Fig. 3.
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$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip]{8899fig5.ps}\end{figure}$	Figure 5: DAOPHOT/ALLSTAR output for G280. Same as Fig. 3.
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