All Figures

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{2173fg1.eps} \end{figure}$ Figure 1: Colour rendition of the data used in this study. The nine UBV WFI frames have been combined to produce an RGB image of the field studied.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{2173fg2.eps} \end{figure}$ Figure 2: Comparison between the magnitudes of Parker (1993) and those of the present work, converted to the standard system. The differences are in the sense $m_{\rm parker} - m_{\rm wfi}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2173fg3a.eps} \includegraphics[width=8cm,clip]{2173fg3b.eps} \end{figure}$ Figure 3: ( Top) The positions in the colour-colour diagram for stars of spectral types earlier than B2, according to Parker's (1993) photometry. ( Bottom) The WFI data, calibrated using Parker's photometry, for the same set of stars. The lines show the reddening trajectories for O3 and B0 stars. The typical errors are smaller than $\pm$ 0.01 for the brighter stars ( upper left-most stars), and approximately $\pm$ 0.04, about twice the size of the symbols for the fainter stars at the lower right.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7cm,clip]{2173fg4a.eps} \includegraphics[width=7cm,clip]{2173fg4b.eps} } \end{figure}$ Figure 4: ( Left) Observed stellar points, together with isochrones for 4.5, 12, and 50 Myr, in the 3-D colour-colour-magnitude stereogram. The theoretical surface is plotted for the 12 Myr isochrone. The tubes representing each isochrone is painted blue, yellow, or red depending on whether the star is of luminosity class V, III, or I respectively. ( Right) Evolutionary track for a 12 $M_\odot$ star. The color of the tube represents the luminosity class, while its width is proportional to the speed at which the star would move during its evolution, representing one measure of the observing probability. Both figures created with VTK (Schroeder et al. 1998).
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In the text

$\begin{figure} \par\includegraphics[width=9.7cm,clip]{2173fg5.eps} \end{figure}$ Figure 5: Comparison of $T_{\rm eff}$ obtained photometrically and spectroscopically. The circles correspond to stars from NGC 2070, the squares to LH104, and the triangles to Hodge 301. Filled symbols represent supergiants, while open symbols are used for all other luminosity classes. The thick line below the diagonal illustrates the effect of a 0.05 blueward shift in (u-b).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2173fg6.eps} \end{figure}$ Figure 6: Photometrically determined HR diagram of the whole region under study.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{2173fg7a.eps} \includegraphics[width=6.6cm,clip]{2173fg7b.eps} \end{figure}$ Figure 7: a) IMF of NGC 2070. The solid and dotted lines represent the best fit to the IMF from Selman et al. (1999), and its 1 $\sigma$ uncertainty. The IMF has been normalized to a 1 Myr burst. b) PDMF, open circles, and IMF, filled circles with error bars, for LH104. The dotted and solid lines represent the best fits to the PDMF in the $12 ~{M}_\odot \le {M} \le 120 ~{M}_\odot$ , and the $12 ~{M}_\odot \le {M} \le 40 ~{M}_\odot$ mass ranges, respectively. The triangles plot the IMF from Testor & Niemela (1998).
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In the text

$\begin{figure} \par\includegraphics[width=6.33cm,clip]{2173fg8a.eps} \includegra... ...]{2173fg8b.eps} \includegraphics[width=6.33cm,clip]{2173fg8c.eps} \end{figure}$ Figure 8: a), ( Top) Field studied in this work identifying several of the OB associations and clusters. Our definition of field is the area outside the marked circles, and within the boundaries of the image. This area has a total size of 0.124 kpc². b), ( Middle) The IMF of the full LMC area covered by Massey (2002), lower line (open triangles), and that obtained by restricting Massey's data to the area covered by this study, upper line (filled triangles). c), ( Bottom) PDMF, open circles, and IMF, filled circle, for the field obtained in this study. The filled triangles correspond to the IMF obtained using data from Massey (2002), restricted to the area of the present study (includes a division by the mass dependent life-time function). The error bars in this latter IMF should be almost the same as those in the IMF of this study, those around the filled circles.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{2173fg9.eps}\par \end{figure}$ Figure 9: HR diagram of the field of the 30 Doradus super-association. The open circles correspond to the values obtained in this work using the Bayesian technique. The filled circles correspond to the stars from Massey (2002) catalogue restricted to our field (his $T_{\rm eff}$ and $M_{\rm bol}$ ). The thick line corresponds to V=12.0.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{2173fg10.eps} \end{figure}$ Figure 10: The large open stars represent non-rotating stars of type B1 V, and B5 V. The open circles represent stars rotating at 80% of the critical speed, for several viewing angles. The reddest point corresponds to the equatorial view, while the bluest to the polar one. Filled circles represent stars rotating at the critical speed. The thick line represents E(U-B)=0.05 normal reddening (after Collins et al. 1991).
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{2173fg1.eps} \end{figure}$	Figure 1: Colour rendition of the data used in this study. The nine UBV WFI frames have been combined to produce an RGB image of the field studied.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{2173fg2.eps} \end{figure}$	Figure 2: Comparison between the magnitudes of Parker (1993) and those of the present work, converted to the standard system. The differences are in the sense $m_{\rm parker} - m_{\rm wfi}$ .
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$\begin{figure} \par\includegraphics[width=9.7cm,clip]{2173fg5.eps} \end{figure}$	Figure 5: Comparison of $T_{\rm eff}$ obtained photometrically and spectroscopically. The circles correspond to stars from NGC 2070, the squares to LH104, and the triangles to Hodge 301. Filled symbols represent supergiants, while open symbols are used for all other luminosity classes. The thick line below the diagonal illustrates the effect of a 0.05 blueward shift in (u-b).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2173fg6.eps} \end{figure}$	Figure 6: Photometrically determined HR diagram of the whole region under study.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{2173fg9.eps}\par \end{figure}$	Figure 9: HR diagram of the field of the 30 Doradus super-association. The open circles correspond to the values obtained in this work using the Bayesian technique. The filled circles correspond to the stars from Massey (2002) catalogue restricted to our field (his $T_{\rm eff}$ and $M_{\rm bol}$ ). The thick line corresponds to V=12.0.
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