$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig1.eps}\end{figure}$ Figure 1: R image of NGC 6192 from the Digitized Sky Survey (DSS). Stars 255, 265 and 274 are identified. North is up and east is to the left.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4716fig2.eps}\end{figure}$ Figure 2: Red giants in NGC 6192, NGC 6208 and NGC 6268 plotted on the unreddened [C₀(45-48),C₀(42-45)] diagram. Solid lines are solar neighbourhood lines for luminosity classes Ib, III and V as defined by Clariá et al. (1994). Cluster members and field stars are represented by filled and open circles, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4716fig3.eps}\end{figure}$ Figure 3: The observed CMD for NGC 6192. The solar metallicity isochrone for log t = 8.25 from Girardi et al. (2000) has been adjusted to E(B-V) = 0.63 and V-M_V = 13.00 (Loktin et al. 2001). The dashed curve is the same isochrone shifted by 0.75 mag to reproduce the upper binary ridge. For the red giants, filled and open circles stand for single and binary members respectively, crosses, for non-members.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig4.eps}\end{figure}$ Figure 4: The observed CMD for NGC 6208. The isochrone for $\log t =$ 9.10 and Z = 0.008 from Girardi et al. (2000) has been adjusted to E(B-V) = 0.32 and V-M_V = 11.15. The dashed curve is the same isochrone shifted by 0.75 mag to reproduce the upper binary ridge. Symbols are as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig5.eps}\end{figure}$ Figure 5: The observed CMD for red evolved stars in NGC 6268. The solar metallicity isochrone for log t = 8.35 from Girardi et al. (2000) has been adjusted to E(B-V) = 0.38 and V-M_V = 11.25. The dashed curve is the same isochrone shifted by 0.75 mag to reproduce the upper binary ridge. Filled and open circles have the same meaning as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig6.eps}\end{figure}$ Figure 6: Galactic coordinates ( l, b) of inner disk open clusters located in the direction of NGC 6192 is.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig7.eps}\end{figure}$ Figure 7: The Galactic plane with the (X, Y) positions of the open clusters located in the direction of NGC 6192. The Carina spiral arm (solid line), the line-of-sight from the Sun to NGC 6192 (straight line) and the position of the Sun are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig8.eps}\end{figure}$ Figure 8: Visual interstellar absorption A_V vs. distance d from the Sun. The relationship corresponding to Baade's window is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig1.eps}\end{figure}$	Figure 1: R image of NGC 6192 from the Digitized Sky Survey (DSS). Stars 255, 265 and 274 are identified. North is up and east is to the left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4716fig2.eps}\end{figure}$	Figure 2: Red giants in NGC 6192, NGC 6208 and NGC 6268 plotted on the unreddened [C₀(45-48),C₀(42-45)] diagram. Solid lines are solar neighbourhood lines for luminosity classes Ib, III and V as defined by Clariá et al. (1994). Cluster members and field stars are represented by filled and open circles, respectively.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig4.eps}\end{figure}$	Figure 4: The observed CMD for NGC 6208. The isochrone for $\log t =$ 9.10 and Z = 0.008 from Girardi et al. (2000) has been adjusted to E(B-V) = 0.32 and V-M_V = 11.15. The dashed curve is the same isochrone shifted by 0.75 mag to reproduce the upper binary ridge. Symbols are as in Fig. 3.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4716fig5.eps}\end{figure}$	Figure 5: The observed CMD for red evolved stars in NGC 6268. The solar metallicity isochrone for log t = 8.35 from Girardi et al. (2000) has been adjusted to E(B-V) = 0.38 and V-M_V = 11.25. The dashed curve is the same isochrone shifted by 0.75 mag to reproduce the upper binary ridge. Filled and open circles have the same meaning as in Fig. 3.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig6.eps}\end{figure}$	Figure 6: Galactic coordinates ( l, b) of inner disk open clusters located in the direction of NGC 6192 is.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig7.eps}\end{figure}$	Figure 7: The Galactic plane with the (X, Y) positions of the open clusters located in the direction of NGC 6192. The Carina spiral arm (solid line), the line-of-sight from the Sun to NGC 6192 (straight line) and the position of the Sun are indicated.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4716fig8.eps}\end{figure}$	Figure 8: Visual interstellar absorption A_V vs. distance d from the Sun. The relationship corresponding to Baade's window is indicated.
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