All Figures

$\begin{figure} \mbox{ \includegraphics[scale=0.35,angle=-90]{4853f1a.ps} \includ... ...11 cm}\includegraphics[scale=0.35,angle=-90]{4853f1x.ps} } \\ \par \end{figure}$ Figure 1: SCUBA images from the survey with detections at both 450 and 850 $\mu$ m. The images displayed here are those discussed further in the text of the paper. Each UC H II region is represented by a pair of images at 450 $\mu$ m (left image) and 850 $\mu$ m (right image). Coordinates are Right Ascension and Declination in the J2000 system. Crosses indicate the positions of ultracompact H II regions from Wood & Churchwell (1989a), Kurtz et al. (1994), Becker et al. (1994) or Giveon et al. (2005). All images have been deconvolved with a model of the JCMT beam to remove the contribution from the error lobe and 450 $\mu$ m images with limited signal-to-noise have been smoothed to the same resolution as the 850 $\mu$ m images to improve the source detections. The full version of this figure is available in electronic form.
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In the text

$\begin{figure} \par\includegraphics*[scale=0.45,trim=110 30 150 50]{4853f3a.ps}\\ \includegraphics*[scale=0.45,trim=110 30 150 50]{4853f3b.ps} \end{figure}$ Figure 3: 850 $\mu$ m SCUBA images of the UC H II field G19.07-0.27 overlaid with countours of MSX 8 $\mu$ m emission ( top) and NVSS 20 cm emission ( bottom). Crosses indicate the position of ultracompact radio components identified from the WC89a, Becker et al. (1994) and Giveon et al. (2005) surveys.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6]{4853f4a.ps} \end{figure}$ Figure 4: Sub-mm "colour-luminosity'' diagram. Radio-loud clumps are indicated by filled circles and radio-quiet clumps are shown by open circles.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f5a.ps} \end{figure}$ Figure 5: Histogram of 850 $\mu$ m clump elongation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f6a.ps} \end{figure}$ Figure 6: Histogram of 850 $\mu$ m clump Y factor (integrated flux divided by peak flux). For an unresolved source the Y-factor is obviously equal to one.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f7a.ps} \end{figure}$ Figure 7: The mean surface density of companions for all the 850 $\mu$ m clumps detected in the survey. Error bars are determined from simple Poisson counting statistics. Solid lines indicate linear least-squared fits to the first 5 and last 3 data points respectively.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,scale=0.6]{4853f8a.ps}\hspace*{2mm} \includegraphics[angle=-90,scale=0.6]{4853f8b.ps} }\end{figure}$ Figure 8: Comparison between the radio to sub-mm ratio ( left: 850 $\mu$ m vs. 2 cm; right: 850 $\mu$ m vs. 6 cm) and the Lyman photon flux inferred from the radio free-free emission of the UC H II regions. Solid lines represent linear least-squared fits to the data. Particular outliers to the fits are indicated and are discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6]{4853f9a.ps} \end{figure}$ Figure 9: The 2 cm to 850 $\mu$ m flux ratio of UC H II regions as a function of distance. Note the trend toward higher values of $S_{850~\mu{\rm m}}/S_{2~{\rm cm}}$ at small distances which may indicate that the 2 cm fluxes of nearby UC H II regions are underestimated due to their over-resolution by the VLA.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f10a.ps} \end{figure}$ Figure 10: Histogram of the angular distance of the UC H II regions to the nearest sub-mm peak (unfilled histogram) plotted over a histogram of the angular distance of the methanol masers from Walsh et al. 2003 to their nearest sub-mm peak (shaded histogram). Note the difference in the two populations in terms of the central peak and the width of the distribution.
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In the text

Full version

$\begin{figure} \mbox{\includegraphics[scale=0.35,angle=-90]{4853of1a.ps} \inclu... ...0.35,angle=-90]{4853of1x.ps} }\\ \par\setcounter{figure}{0} \par \end{figure}$ Figure 1: SCUBA images from the survey with detections at both 450 and 850 $\mu$ m. Each UC H II region is represented by a pair of images at 450 $\mu$ m (left image) and 850 $\mu$ m (right image). Coordinates are Right Ascension and Declination in the J2000 system. Crosses indicate the positions of ultracompact H II regions from Wood & Churchwell (1989a), Kurtz et al. (1994), Becker et al. (1994) or Giveon et al. (2005). All images have been deconvolved with a model of the JCMT beam to remove the contribution from the error lobe and 450 $\mu$ m images with limited signal-to-noise have been smoothed to the same resolution as the 850 $\mu$ m images to improve the source detections.
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In the text

$\begin{figure} \mbox{\includegraphics[scale=0.35,angle=-90]{4853of1y.ps} \inclu... ...=0.35,angle=-90]{4853of1av.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\mbox{\includegraphics[scale=0.35,angle=-90]{4853of1aw.ps} \includ... ...e=0.35,angle=-90]{4853of1bt.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\mbox{ \includegraphics[scale=0.35,angle=-90]{4853of1bu.ps} \inclu... ...e=0.35,angle=-90]{4853of1cr.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\mbox{ \hspace*{0.11cm}\includegraphics[scale=0.35,angle=-90]{4853... ...=0.35,angle=-90]{4853of1dp.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\mbox{\hspace*{0.11cm}\includegraphics[scale=0.35,angle=-90]{4853o... ...e=0.35,angle=-90]{4853of1ed.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \mbox{ \includegraphics[scale=0.35,angle=-90]{4853f2a.ps} \includ... ...e=0.35,angle=-90]{4853f2x.ps} }\\ \par\setcounter{figure}{1} \par \end{figure}$ Figure 2: SCUBA images of the ultracompact H II regions in the survey with detections at 850 $\mu$ m only. Each UC H II region is represented by a pair of images at 450 $\mu$ m (left image) and 850 $\mu$ m (right image). Coordinates are Right Ascension and Declination in the J2000 system. Crosses indicate the positions of ultracompact H II regions from Wood & Churchwell (1989a), Kurtz et al. (1994), Becker et al. (1994) or Giveon et al. (2005). All images have been deconvolved with a model of the JCMT beam to remove the contribution from the error lobe.
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In the text

$\begin{figure} \par\includegraphics[scale=0.45,trim=110 30 150 50]{4853f3a.ps}\\ \includegraphics[scale=0.45,trim=110 30 150 50]{4853f3b.ps} \end{figure}$	Figure 3: 850 $\mu$ m SCUBA images of the UC H II field G19.07-0.27 overlaid with countours of MSX 8 $\mu$ m emission ( top) and NVSS 20 cm emission ( bottom). Crosses indicate the position of ultracompact radio components identified from the WC89a, Becker et al. (1994) and Giveon et al. (2005) surveys.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6]{4853f4a.ps} \end{figure}$	Figure 4: Sub-mm "colour-luminosity'' diagram. Radio-loud clumps are indicated by filled circles and radio-quiet clumps are shown by open circles.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f5a.ps} \end{figure}$	Figure 5: Histogram of 850 $\mu$ m clump elongation.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f6a.ps} \end{figure}$	Figure 6: Histogram of 850 $\mu$ m clump Y factor (integrated flux divided by peak flux). For an unresolved source the Y-factor is obviously equal to one.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f7a.ps} \end{figure}$	Figure 7: The mean surface density of companions for all the 850 $\mu$ m clumps detected in the survey. Error bars are determined from simple Poisson counting statistics. Solid lines indicate linear least-squared fits to the first 5 and last 3 data points respectively.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,scale=0.6]{4853f8a.ps}\hspace*{2mm} \includegraphics[angle=-90,scale=0.6]{4853f8b.ps} }\end{figure}$	Figure 8: Comparison between the radio to sub-mm ratio ( left: 850 $\mu$ m vs. 2 cm; right: 850 $\mu$ m vs. 6 cm) and the Lyman photon flux inferred from the radio free-free emission of the UC H II regions. Solid lines represent linear least-squared fits to the data. Particular outliers to the fits are indicated and are discussed in the text.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6]{4853f9a.ps} \end{figure}$	Figure 9: The 2 cm to 850 $\mu$ m flux ratio of UC H II regions as a function of distance. Note the trend toward higher values of $S_{850~\mu{\rm m}}/S_{2~{\rm cm}}$ at small distances which may indicate that the 2 cm fluxes of nearby UC H II regions are underestimated due to their over-resolution by the VLA.
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$\begin{figure} \par\includegraphics[angle=-90,scale=0.6,clip]{4853f10a.ps} \end{figure}$	Figure 10: Histogram of the angular distance of the UC H II regions to the nearest sub-mm peak (unfilled histogram) plotted over a histogram of the angular distance of the methanol masers from Walsh et al. 2003 to their nearest sub-mm peak (shaded histogram). Note the difference in the two populations in terms of the central peak and the width of the distribution.
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$\begin{figure} \mbox{\includegraphics[scale=0.35,angle=-90]{4853of1y.ps} \inclu... ...=0.35,angle=-90]{4853of1av.ps} }\\ \par\setcounter{figure}{0} \par\end{figure}$	Figure 1: continued.
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