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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1a.ps} \end{figure}$ Figure 1: Stellar surface density contour plots for the 54 embedded clusters produced with a bin size of 80 $\hbox {$^{\prime \prime }$ }$ (step size = 40 $^{\prime \prime }$ ). The star symbol represents the position of the luminous IRAS source. Contours begin at mode+2 $\sigma$ level and increase in steps of 1 $\sigma$ , $\sigma$ being the average noise measured over the an area of $600\hbox {$^{\prime \prime }$ }\times 600\hbox {$^{\prime \prime }$ }$ centered on each target. The dots represent the point sources with phqual = A, B, C, D catalogued in the 2MASS GATOR database. The full figure is available at http://www.edpsciences.org/.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3104fig2.ps} \end{figure}$ Figure 2: Embedded cluster mass distribution function. The dotted line represent the ECMDF from LL03 for the embedded clusters within 2 kpc distance. The solid line shows the ECMDF for the clusters from this work.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3104fig3.ps} \end{figure}$ Figure 3: A plot of the mass of the associated clusters vs. the luminosity of the target massive protostar.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3104fig4.ps} \end{figure}$ Figure 4: Color-color diagram of NIR counterparts to the 1.2 mm peaks of HMPOs. The solid curve represents the HAeBe curve by Lada & Adams (1992), thick-solid curve represents the main-sequence tracks, the dotted line shows the T-Tauri locus from Meyer et al. (1997) and the dashed lines represent the reddening vectors. The dots represent the point sources from GATOR PSC and star symbols represent the extended sources from the GATOR XSC.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{3104fig5.ps} \end{figure}$ Figure 5: An HR-diagram showing evolutionary tracks for massive stars that are gaining mass by accretion. The zero age main sequence (ZAMS) line is shown annotated by stellar mass in solar masses. The four evolutionary tracks are for stars accreting with rates ( $\dot{M}$ ) that vary as a power law of stellar mass (M), with indexes 0.5, 1, 1.5 and 2 ( bottom to top respectively). $t_{\rm ZAMS}$ indicates the time spent on the ZAMS line for a 4 $M_{\odot }$ star before it deviates off the line. The accretion rate at the time of deviation, which is also the maximum accretion rate for that track is marked below each track.
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In the text

Full version

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1b.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1c.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1d.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1e.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3104fig2.ps} \end{figure}$	Figure 2: Embedded cluster mass distribution function. The dotted line represent the ECMDF from LL03 for the embedded clusters within 2 kpc distance. The solid line shows the ECMDF for the clusters from this work.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3104fig3.ps} \end{figure}$	Figure 3: A plot of the mass of the associated clusters vs. the luminosity of the target massive protostar.
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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{3104fig1b.ps}\end{figure}$	Figure 1: continued.
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