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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fig1.eps}\end{figure}$ Figure 1: Simulated line shapes for a cluster of 30 UCHII regions, as described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{Fig2.eps}\end{figure}$ Figure 2: The Brackett line profiles of the RISN in NGC 5253, from Turner et al. (2003). The small ( $0.001~\mu$ m) ticks equal 74 km s^-1. This RISN has only the narrow component.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fig3.eps}\end{figure}$ Figure 3: Simulated line shapes for a cluster of 30 UCHII regions and 5 WR stars, as described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{Fig4.eps}\end{figure}$ Figure 4: Brackett line profiles of two RISN in He 2-10, from Henry et al. (2007). Intensity is relative to peak. These have both narrow and wide components.
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In the text