All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig1.ps} \end{figure}$ Figure 1: Ionization front (IF) "chord diameter'' (diameter of a circle fitted to the contour of plus $\sim$ 30% the average background intensity), as a function of the projected distance to the main ionizing star in the Trapezium cluster, $\theta {^{1}}$ Ori C. The different symbols represent the proplyds that are ionized primarily by the stars indicated in the plot legend. For example, the largest bright proplyd 244-440 is being ionized by both $\theta {^{1}}$ Ori C and $\theta ^{2}$ Ori A. There are 2 proplyds (252-457; 282-458) being ionized by both $\theta ^{2}$ Ori B, the bright star in the east direction from $\theta ^{2}$ Ori A, and $\theta {^{1}}$ Ori C.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig2.ps} \end{figure}$ Figure 2: Diameter ratio, R = disk diameter/ IF diameter, as a function of the disk diameter in pixels. The gray (yellow) band represents the average and dispersion of the sample (49 $\pm$ 16%).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig3.ps} \end{figure}$ Figure 3: Spatial distribution of the 10 proplyds with embedded silhouette disks. The black filled circles represent the silhouette disks and the colored, open circles represent the ionization fronts. Green is for the proplyds ionized primarily by $\theta {^{1}}$ Ori C (072-135; 163-222; 181-247; 182-413), blue for the proplyds ionized by $\theta ^{2}$ Ori A (176-543; 206-446) and red for proplyds ionized by both stars (141-520; 143-522; 197-427; 244-440). The circle diameters are proportional to the true disk and IF diameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig4.ps} \end{figure}$ Figure 4: Spatial distribution of total sample of 149 disks in the Trapezium cluster. The "star'' symbols represent the 6 brightest OB stars. The filled circles indicate the positions of the 135 bright proplyds' disks; gray (green) for the 10 proplyds with embedded silhouette disks and black for the remaining 125 from which the disk diameter is 49% of the correspondant IF diameter. The unfilled circles represent the positions of the 14 pure silhouettes.The diameters of the circles are proportional to the disk diameters they represent.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig5.ps} \end{figure}$ Figure 5: Disk diameter distribution for the total sample of 149 proplyds. The gray (green) filled histogram represents the 135 bright proplyds disks - 10 dark disks embedded in the bright proplyds' cusps and 125 disks derived from the cusps diameters. The black filled histogram represents the 14 pure silhouettes seen only against the Orion Nebula background. The first bin (0-100 AU) is highly incomplete due to the resolution limit of the data. The virtual sample, in dashed line, was estimated based on the L-band excess of Trapezium sources. The large silhouettes 218-354 and 114-426 are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig6.ps} \end{figure}$ Figure 6: Power-law fit to the size distribution of disks for diameters between 100-400 AU. The data can be described by a power-law with an exponent of -1.9 $\pm$ 0.3.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig7.ps} \end{figure}$ Figure 7: Cumulative function of the histogram. The real sample is composed by the 149 disks in this paper and represents $\sim$ 50% of all Trapezium's YSO observed with the HST. The virtual sample is the corrected sample accounting for the 35% of HST unresolved disks and is composed by our sample corrected by adding 106 disks with diameters less than 50 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig8.ps} \end{figure}$ Figure 8: Disk diameter versus spectral-type of central parent star. There is not an obvious correlation between the two variables.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig2.ps} \end{figure}$	Figure 2: Diameter ratio, R = disk diameter/ IF diameter, as a function of the disk diameter in pixels. The gray (yellow) band represents the average and dispersion of the sample (49 $\pm$ 16%).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig6.ps} \end{figure}$	Figure 6: Power-law fit to the size distribution of disks for diameters between 100-400 AU. The data can be described by a power-law with an exponent of -1.9 $\pm$ 0.3.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig7.ps} \end{figure}$	Figure 7: Cumulative function of the histogram. The real sample is composed by the 149 disks in this paper and represents $\sim$ 50% of all Trapezium's YSO observed with the HST. The virtual sample is the corrected sample accounting for the 35% of HST unresolved disks and is composed by our sample corrected by adding 106 disks with diameters less than 50 AU.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3540fig8.ps} \end{figure}$	Figure 8: Disk diameter versus spectral-type of central parent star. There is not an obvious correlation between the two variables.
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