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$\begin{figure} \par\includegraphics[angle=90,width=10cm,clip]{Fig1.eps} \end{figure}$ Figure 1: Colour-coded image of the entire G9.62+0.19 region taken in the three broad-band NIR filters J (blue), H (green), and $K_{\rm s}$ (red). The large-scale contour lines denote the emission levels derived from the 8.28 $\mu$ m image of the related MSX source. The left-most large contour line indicates the position of the close-by Infrared Dark Cloud.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig2CMJN.eps} \end{figure}$ Figure 2: Cutout of the central region of Fig. 1. The overlaid contour lines denote the 3.6 cm emission of the ionized regions as measured by Testi et al. (2000). The source annotation follows their nomenclature. Note that also component F features weak 3.6 cm emission - the related contour line merges with the seeing disk of the yellow star. The black cross marks the peak of the NH₃(5, 5) HMC emission (Hofner et al. 1994).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig3.eps} \end{figure}$ Figure 3: The same field of view as in Fig. 2, but now the overlaid contour lines trace the thermal NH₃(5, 5) emission of the HMC as measured by Hofner et al. (1994). The ellipse in the lower left corner indicates the size of the synthesized VLA beam. The black cross at the reference position marks the faint peak of the 3.6-cm HMC emission (Testi et al. 2000).
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In the text

$\begin{figure} \par\includegraphics[width=4.2cm,clip]{Fig4a.eps}\hspace*{3mm} \... ...e.eps}\hspace*{3mm} \includegraphics[width=4.2cm,clip]{Fig4f.eps} \end{figure}$ Figure 4: Cutout gallery showing the four objects of the HMC region G9.62+0.19-F. Upper row from left to right: H, $K_{\rm s}$ , L' band. Lower row from left to right: nb_M, N1, 11.7 $\mu$ m. The size of the cutout box is ca. $5\hbox{$.\!\!^{\prime\prime}$ }4 \times 5\hbox{$.\!\!^{\prime\prime}$ }4$ . While the foreground star (F2) quickly fades towards longer wavelengths, another object very close to it (F4) gets stronger and finally dominates the region. We presume that it is a potential trace of the HMC whose location is here indicated by the upper contours of the NH₃(5, 5) emission. While all the other images are taken from the plain imaging data, the N1 image at 8.7 $\mu$ m shows the TIMMI2 data after deconvolution with the standard star HD 169916. Note that the smaller spots in that particular image are deconvolution artefacts that change their position and strength when the deconvolution parameters are varied.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fig5.eps} \end{figure}$ Figure 5: Inverse gray-scale representation of the 11.7 $\mu$ m SpectroCam-10 image displaying a smaller cutout of the G9.62+0.19 region. The weaker but nevertheless clearly visible spot to the east represents emission from the region of the HMC component F and arises probably from object F4 (see also Fig. 4). Overlaid are the 1.3 cm continuum VLA contours from Cesaroni et al. (1994). The compact radio source to the south-east of the compact MIR emission is the UCH II region G9.62+0.19 D.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig6.eps} \end{figure}$ Figure 6: The ${\it JHK}_{\rm s}$ colour composite, overlaid with the TIMMI2 N1 band data as contours. The bright source at the offset coordinates (-16, 14) served as main astrometric reference for the TIMMI2 data.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig7.eps} \end{figure}$ Figure 7: This image shows G9.62+0.19 in the K narrow-band filters: Br $~ \gamma$ (blue), H₂ (red), (Br $\gamma$ + H₂)/2 (green). The Br $~ \gamma$ emission arises mainly from the compact H II region G9.62+0.19 B. Note that the H₂ emission blob roughly in the image centre has its own substructure. The diffuse emission to the north of it (white) turns out to be mainly scattered light (see Fig. 8).
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{Fig8.eps} \end{figure}$ Figure 8: Polarisation map overlaid over an image of Stokes-I (i.e. the intensity) of G9.62+0.19, both measured at 2.09 $\mu$ m. We binned the data to a pixel size of $0 \hbox{$.\!\!^{\prime\prime}$ }6 \times 0 \hbox{$.\!\!^{\prime\prime}$ }6$ before deriving the polarisation. The ellipse is an indicator for the location of the illuminator whose scattered light causes the high degree of linear polarisation in some parts of the image (see Sect. 3.5 for details). The thick crosses mark the positions of the hypercompact H II regions E, G, H, and I (cf. Fig. 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fig9.eps} \end{figure}$ Figure 9: Example for the appearance of the SED of a hot molecular core, calculated with a radiative transfer model (solid line). For this graph we used a central heating source with $T_{{\rm eff}} = 22~500$ K and a total luminosity of $1.88 \times 10^4$ $L_{\odot }$ . The total mass contained in the model space was 95 $M_{\odot }$ . For this particular model we assumed a constant density distribution and an outer radius of 2600 AU. No accretion luminosity was added. The drawn-in symbols indicate the fluxes we measure for the objects F1 (plus-signs) and F4 (crosses), respectively. The asterisk at 8.7 $\mu$ m denotes the integrated flux from an area covering both F1 and F4. The 2.7 mm flux from Hofner et al. (1996) is marked by a small square. As comparison, a 90 K modified blackbody is plotted as a dashed line. However, the significance of such a temperature is put into perspective in Sect. 4.1.1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{Fig10.eps} \end{figure}$ Figure 10: The K band medium-resolution spectrum of object F1 (in arbitrary units), taken with SOFI at the ESO NTT.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=10cm,clip]{Fig1.eps} \end{figure}$	Figure 1: Colour-coded image of the entire G9.62+0.19 region taken in the three broad-band NIR filters J (blue), H (green), and $K_{\rm s}$ (red). The large-scale contour lines denote the emission levels derived from the 8.28 $\mu$ m image of the related MSX source. The left-most large contour line indicates the position of the close-by Infrared Dark Cloud.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig3.eps} \end{figure}$	Figure 3: The same field of view as in Fig. 2, but now the overlaid contour lines trace the thermal NH₃(5, 5) emission of the HMC as measured by Hofner et al. (1994). The ellipse in the lower left corner indicates the size of the synthesized VLA beam. The black cross at the reference position marks the faint peak of the 3.6-cm HMC emission (Testi et al. 2000).
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$\begin{figure} \par\includegraphics[width=14cm,clip]{Fig6.eps} \end{figure}$	Figure 6: The ${\it JHK}_{\rm s}$ colour composite, overlaid with the TIMMI2 N1 band data as contours. The bright source at the offset coordinates (-16, 14) served as main astrometric reference for the TIMMI2 data.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{Fig10.eps} \end{figure}$	Figure 10: The K band medium-resolution spectrum of object F1 (in arbitrary units), taken with SOFI at the ESO NTT.
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