\relax 
\@writefile{toc}{\contentsline {section}{\numberline {1.}Introduction}{363}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Colour--magnitude diagram of R136 for all stars measured in the combined images with photometric errors smaller than 0.2 magnitudes in both filters.}}{364}}
\newlabel{cmd}{{1}{364}}
\@writefile{toc}{\contentsline {section}{\numberline {2.}Observations}{364}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Radial star-density distribution for the two different populations. The solid line shows the stars with ${\rm  F555W}-{\rm  F814W} < 1.1$, while the dashed line show the distribution of stars with redder colours. Due to the high number of saturated stars in the core of R136, the first bin (0--2$''$) is severely affected by incompleteness.}}{365}}
\newlabel{spat}{{2}{365}}
\@writefile{toc}{\contentsline {section}{\numberline {3.}Age and Mass}{365}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Pre-main-sequence isochrones for ages 10$^{6}$--10$^{7}$\nobreakspace  {}yr (Bernasconi 1996), superposed on the dereddened CMD.}}{366}}
\newlabel{iso}{{3}{366}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces HR diagram, with theoretical pre-main-sequence evolutionary tracks from Bernasconi (1996) superposed for masses in the range 0.8--7$M_{\odot }$. Dashed lines mark different completeness regions. }}{367}}
\newlabel{hr}{{4}{367}}