Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{fig1.cmd.ps} \end{figure}$ Figure 1: Colour-magnitude diagram of the WLM field, stars with colour errors <0.10 are plotted.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{fig2.cc.ps} \end{figure}$ Figure 2: Colour-colour diagram showing the boxes of C stars and M stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90, width=12.1cm]{fig3.map.eps} \end{figure}$ Figure 3: The WLM field, carbon stars identified in this study are represented by big dots. Small dots correspond to stars plotted in Fig. 1. The limit of the galaxy, as determined from star counts, is outlined, see Sect. 4.2. The HST field investigated by Dolphin (2000), well within this ellipse, is also traced. This figure does not represent the whole area surveyed, a 14' wide band further south is not shown. One of the gaps between CCDs is quite obvious in the high density central part of WLM. North is on top, East is on the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig4.his.ps} \end{figure}$ Figure 4: Luminosity function of the C stars in WLM. A Gaussian with a $\sigma$ = 0.3 is eye-fitted to the data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig5.den.ps} \end{figure}$ Figure 5: Isodensity contours of the stellar content of WLM. This figure is based on our photometry to $I \approx 22$ . The size of the area represented is 25.7' $\times$ 25.5'. The values of each contour are 9, 33, 45, 78, 111, 145, and 178 stars per arcmin².
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig6.majorprof.ps} \end{figure}$ Figure 6: Folded density profile along the major axis of WLM. The solid line corresponds to the running-mean (weights: 0.2, 0.3, 0.3, 0.2) of the data points. The dashed line represents the foreground density well established from counts far from WLM.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig7.minorprof.ps} \end{figure}$ Figure 7: Folded density profile along the minor axis of WLM. The solid line corresponds to the running-mean (weights: 0.2, 0.3, 0.3, 0.2) of the data points. The dashed line represents the foreground density well established from counts far from WLM.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig8.power.ps} \end{figure}$ Figure 8: Surface density profiles of red stars (solid dots) and C stars (open circles) have similar scale lengths. The dashed lines are least square fits through the outer points. To facilitate the comparison, 2 is added to the ln ( $\rho$ ) of C stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig9.rRI.ps}\end{figure}$ Figure 9: The distance of stars from the major axis are plotted in term of their colours. We distinguish three populations: the blue stars concentrated closer to the center, the RGB and C stars (big dots) which occupy a larger volume.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig10.2his.ps} \end{figure}$ Figure 10: Colour distribution of the AGB M stars within the ellipse (solid line) and outside the ellipse (dashed line), scaled to match the area of the ellipse.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{fig1.cmd.ps} \end{figure}$	Figure 1: Colour-magnitude diagram of the WLM field, stars with colour errors <0.10 are plotted.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{fig2.cc.ps} \end{figure}$	Figure 2: Colour-colour diagram showing the boxes of C stars and M stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig4.his.ps} \end{figure}$	Figure 4: Luminosity function of the C stars in WLM. A Gaussian with a $\sigma$ = 0.3 is eye-fitted to the data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig5.den.ps} \end{figure}$	Figure 5: Isodensity contours of the stellar content of WLM. This figure is based on our photometry to $I \approx 22$ . The size of the area represented is 25.7' $\times$ 25.5'. The values of each contour are 9, 33, 45, 78, 111, 145, and 178 stars per arcmin².
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig6.majorprof.ps} \end{figure}$	Figure 6: Folded density profile along the major axis of WLM. The solid line corresponds to the running-mean (weights: 0.2, 0.3, 0.3, 0.2) of the data points. The dashed line represents the foreground density well established from counts far from WLM.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig7.minorprof.ps} \end{figure}$	Figure 7: Folded density profile along the minor axis of WLM. The solid line corresponds to the running-mean (weights: 0.2, 0.3, 0.3, 0.2) of the data points. The dashed line represents the foreground density well established from counts far from WLM.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig8.power.ps} \end{figure}$	Figure 8: Surface density profiles of red stars (solid dots) and C stars (open circles) have similar scale lengths. The dashed lines are least square fits through the outer points. To facilitate the comparison, 2 is added to the ln ( $\rho$ ) of C stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig9.rRI.ps}\end{figure}$	Figure 9: The distance of stars from the major axis are plotted in term of their colours. We distinguish three populations: the blue stars concentrated closer to the center, the RGB and C stars (big dots) which occupy a larger volume.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig10.2his.ps} \end{figure}$	Figure 10: Colour distribution of the AGB M stars within the ellipse (solid line) and outside the ellipse (dashed line), scaled to match the area of the ellipse.
Open with DEXTER