All Figures

$\begin{figure} \par {\psfig{file=Boeche_fig_1.ps,width=8.8cm} }\end{figure}$ Figure 1: Finding chart for NGC 6913 program stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{Boeche_fig_2.ps} \end{figure}$ Figure 2: The program stars on the reddening corrected V₀, (B-V)₀ diagram using E_B-V from Table 3 and V, B-V photometry from Table 1 for R_V=A_V/E_B-V=3.6 appropriate for NGC 6913 according to Johnson (1962). The isochrone for solar metallicity and 5 Myr is from Bertelli et al. (1994) and it is scaled to m-M=10.5(dotted line), m-M=11.0 (solid line) and m-M=11.7 (dashed line). It is evident how the cluster distance cannot be well constrained. In this paper we adopt a 1.6 kpc distance.
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{Boeche_fig_3.ps} }\end{figure}$ Figure 3: Orbital solutions for the binary program stars (cf. Table 6).
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In the text

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_4.ps} } \end{figure}$ Figure 4: Comparison between Dias et al. (2002) and Sanders (1973) membership data for the 24 stars in common.
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In the text

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_5.ps} } \end{figure}$ Figure 5: Radial velocity distribution of the program stars. A Gaussian with center at $RV_\odot =-16.9$ km s^-1 and $\sigma =2.0$ km s^-1 fits the member stars. Shaded elements represent stars which radial velocity differs by more than 3 $\sigma$ from the cluster mean velocity.
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In the text

$\begin{figure} \par {\includegraphics[width=17.8cm,clip]{Boeche_fig_6.ps} } \end{figure}$ Figure 6: Comparison of a 30 $^{\prime }\times 30^{\prime }$ field from POSS-II (top left) and IRAS 100 $\mu$ m wavelength image (bottom left) centered on NGC 6913. Stellar surface density of the same stellar field is obtained from USNO-A2.0 optical catalog (top right) with minimum and maximum density of 0.5 and 4.7 stars/arcmin² (clearest and darkest zone) respectively and grey levels in step of 0.25 stars/arcmin², and from 2MASS infrared catalog (bottom right) with minimum and maximum density of 6.9 and 14.2 stars/arcmin² (clearest and darkest zone) respectively and grey levels in step of 0.5 stars/arcmin².
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In the text

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_7.ps} } \end{figure}$ Figure 7: Mass function of the cluster NGC 6913 as it results from the spectral classification of the member stars. The dashed line is a fit with a Salpeter law N(m)=489 m^-2.35 to O and B stars ( $M\geq 6$ $M_\odot$ ).
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In the text

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_8.ps} } \end{figure}$ Figure 8: Member stars of NGC 6913 with mass smaller (left) and larger (right) then 6 $M_\odot$ . Massive stars show a clear clustering while the lighter seem randomly distributed.
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In the text

$\begin{figure} \par {\psfig{file=Boeche_fig_1.ps,width=8.8cm} }\end{figure}$	Figure 1: Finding chart for NGC 6913 program stars.
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$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{Boeche_fig_3.ps} }\end{figure}$	Figure 3: Orbital solutions for the binary program stars (cf. Table 6).
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$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_4.ps} } \end{figure}$	Figure 4: Comparison between Dias et al. (2002) and Sanders (1973) membership data for the 24 stars in common.
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$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_5.ps} } \end{figure}$	Figure 5: Radial velocity distribution of the program stars. A Gaussian with center at $RV_\odot =-16.9$ km s^-1 and $\sigma =2.0$ km s^-1 fits the member stars. Shaded elements represent stars which radial velocity differs by more than 3 $\sigma$ from the cluster mean velocity.
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$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_7.ps} } \end{figure}$	Figure 7: Mass function of the cluster NGC 6913 as it results from the spectral classification of the member stars. The dashed line is a fit with a Salpeter law N(m)=489 m^-2.35 to O and B stars ( $M\geq 6$ $M_\odot$ ).
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$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{Boeche_fig_8.ps} } \end{figure}$	Figure 8: Member stars of NGC 6913 with mass smaller (left) and larger (right) then 6 $M_\odot$ . Massive stars show a clear clustering while the lighter seem randomly distributed.
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