Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{aa1565f1.ps} \end{figure}$ Figure 1: Schematic representation of the five TNG fields relative to the CFH12K fields. Dots are the known C stars; crosses are the newly discovered C stars; the dashed line corresponds to the major axis of the disk of M 31. The cluster G1 is represented by a circle, the triangle is the region called G1 field and the ellipse outlines the Ferguson et al. (2002) clump (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{aa1565f2.ps} \end{figure}$ Figure 2: The colour-magnitude diagrams of the five fields under investigation. Only stars with colour errors <0.100 are plotted.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{aa1565f3.ps} \end{figure}$ Figure 3: The AGB star region is outlined on the CMD of the concatenated five fields.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{aa1565f4.ps} \end{figure}$ Figure 4: The number of AGB stars in the 88 arcmin² region along the major axis of M 31. The dashed line represents Durrell's et al. (2001) counts in R1.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{aa1565f5.ps} \end{figure}$ Figure 5: The colour-colour diagrams of the five fields. Only stars with $\sigma _{{\rm colours}}<0.125$ are plotted (see text). The two boxes define the samples of C and M stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{aa1565f6.ps} \end{figure}$ Figure 6: Luminosities of C stars from Battinelli et al. (2003) (open circles) and from the present paper (filled triangles) as a function of the angular distance from the M 31 center. The straight line is the least square fit to the Battinelli et al. C stars. The upper panel presents the reddening corrected I magnitudes while the lower panel shows the bolometric magnitudes.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{aa1565f1.ps} \end{figure}$	Figure 1: Schematic representation of the five TNG fields relative to the CFH12K fields. Dots are the known C stars; crosses are the newly discovered C stars; the dashed line corresponds to the major axis of the disk of M 31. The cluster G1 is represented by a circle, the triangle is the region called G1 field and the ellipse outlines the Ferguson et al. (2002) clump (see text for details).
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{aa1565f2.ps} \end{figure}$	Figure 2: The colour-magnitude diagrams of the five fields under investigation. Only stars with colour errors <0.100 are plotted.
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$\begin{figure} \par\includegraphics[width=5.7cm,clip]{aa1565f3.ps} \end{figure}$	Figure 3: The AGB star region is outlined on the CMD of the concatenated five fields.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{aa1565f4.ps} \end{figure}$	Figure 4: The number of AGB stars in the 88 arcmin² region along the major axis of M 31. The dashed line represents Durrell's et al. (2001) counts in R1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{aa1565f5.ps} \end{figure}$	Figure 5: The colour-colour diagrams of the five fields. Only stars with $\sigma _{{\rm colours}}<0.125$ are plotted (see text). The two boxes define the samples of C and M stars.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{aa1565f6.ps} \end{figure}$	Figure 6: Luminosities of C stars from Battinelli et al. (2003) (open circles) and from the present paper (filled triangles) as a function of the angular distance from the M 31 center. The straight line is the least square fit to the Battinelli et al. C stars. The upper panel presents the reddening corrected I magnitudes while the lower panel shows the bolometric magnitudes.
Open with DEXTER