All Figures

$\begin{figure} \par\includegraphics[height=7.65cm,width=7.8cm,clip]{0890fig1.ps}\includegraphics[height=7.65cm,width=7.85cm,clip]{0890fig2.ps}\end{figure}$ Figure 1: Left panel: 1.2 mm SIMBA/SEST contours overlaid on the grayscale ISAAC Ks-band image. The contour levels correspond to (5, 10, 20, 40, 60, 80, 110) $\times$ 46 mJy/beam. The inverted gray scale ISAAC Ks image shows the stellar population and the short-wavelength nebulosity. Right Panel: high sensitivity MSX 8.28 $\mu$ m contours, showing an extended, continuous distribution of warm dust in the star-forming region. The contours mark 5, 10, 50, 100, 150, 250, 300 $\sigma$ levels; the MSX point source flux is 30.74 Jy. The square marks the radio position of the UC H II region G268.42-0.85, while the ellipse indicates the positional error ellipse of the IRAS point source 09002-4732. The MSX A-band images are probably influenced by PAH emission and this explains the offset between the IRAS- and MSX-peaks.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0890fig3.ps}\end{figure}$ Figure 2: MEM deconvolved CS J=7-6 contours (vel. channel 2.75 km s^-1, Lapinov et al. 1998) overlaid over the central region of the inverted Ks-band ISAAC image. The CS J=7-6 line transition shows two clumps with only a small line-of-sight velocity difference. The gray scale Ks-image suggests that the SE clump is located in front of the cluster while the NW clump is located behind the embedded stars. The squares mark stars with NIR excess larger than 0.1 mag. The large rectangle marks the approximate field of view of the CS observations, while the thin contours mark the free-free emission morphology (Walsh et al. 1998).
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In the text

$\begin{figure} \par\includegraphics[width=13cm]{0890fig4.eps}\end{figure}$ Figure 3: False-colour composite image from the near-infrared observations. The Ks band image is coded in red, H in green and Js in blue.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0890fig5.ps}\end{figure}$ Figure 4: Js-band surface brightness of the reflection nebulosity versus the distance from the UC H II region G268.42-0.85 plotted on a logarithmic scale. The best fit gives an $R^{-1.4 \pm 0.2}$ dependence.
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In the text

$\begin{figure} \par\includegraphics[height=18.3cm,width=13cm]{0890fig6.eps} % \end{figure}$ Figure 5: Outlines of the filamentary structure of extincting material seen in the NIR images. The solid lines trace the general structure, while the dashed lines indicate the dark filaments (S1-S5). The dense globules inside the filaments are indicated with hatched ellipses and designated as G1-G15. The two circles (IS1 and IS2) mark two isolated silhouette objects.
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In the text

$\begin{figure} \par\includegraphics[height=7.1cm,width=7.1cm,clip]{0890fig7.ps}\end{figure}$ Figure 6: Unsharp-masked magnified field from Fig. 5 showing the objects IS1 and IS2.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0890fig8.eps}\end{figure}$ Figure 7: Ks-band inverted gray scale image. Crosses mark the 1106 stars identified in the Ks band, while boxes denoted those with identified infrared excess emission.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0890fig9.ps}\end{figure}$ Figure 8: Colour-colour diagram of the stellar population around IRAS 09002-4732. The colour index ( $J{\rm s}-H$ ) is plotted against the (H-Ks) index. The connected crosses indicate the colours of unreddened main sequence stars (Bessell & Brett 1988; Wegner 1994). Single crosses show the observed colours, while the asterisks represent stars with NIR excess larger than 0.1 mag. The dashed lines enclose the possible colours of reddened main sequence stars. The solid line represents the T Tauri locus (Meyer et al. 1997). The mean error is plotted in the figure legend.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{0890fig10.ps}\end{figure}$ Figure 9: Near-infrared colour-magnitude diagram of the same stellar population as in Fig. 8. The symbols are identical to those used in Fig. 8. The assumed distance of the zero age main sequence stars is 1.3 kpc. Individual error bars are shown on each object, some of which are smaller than the actual symbols.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0890fig11.ps}\end{figure}$ Figure 10: The distribution of the stellar detections as a function of colour. The dashed line traces the histrogram of stellar detections in all three near-infrared bands, while the solid line shows the distribution of stars with identified infrared excess emission. The reddening shows a well-defined peak at $J{\rm s}-K$ s $\simeq$ 2.7 for both stellar populations, and a peak at $J{\rm s}-K$ s $\simeq$ 1.6 for the main-sequence stars.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0890fig12.ps}\end{figure}$ Figure 11: Ks-band stellar density derived from stellar counts in concentric annuli around the UC H II region G268.42-0.85.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0890fig13.ps}\end{figure}$ Figure 12: The morphology of the UC H II region G268.45-0.85 as seen in 2.2 $\mu$ m (Ks), 3.78 $\mu$ m (L), 4.66 $\mu$ m (M), 4.07 $\mu$ m (Br $\alpha$ ), 11.9 $\mu$ m (N11.9) and 12.9 $\mu$ m (N12.9) images. The overlaid contours are 8.64 GHz radio continuum measurements from Walsh et al. (1998). The objects of particular interest are marked with letters from A-I. The resolution of the images are as follows $d(K{\rm s})\simeq 0.44\hbox {$^{\prime \prime }$ }=600$ AU, $d(L)\simeq 0.45\hbox {$^{\prime \prime }$ }= 590$ AU, $d(4.07~\mu{\rm m})\simeq 0.6\hbox{$^{\prime\prime}$ }=780$ AU, $d(M)\simeq 0.47\hbox {$^{\prime \prime }$ }= 610$ AU, $d(11.9~\mu{\rm m}, 12.9~\mu{\rm m})\sim 0.8\hbox{$^{\prime\prime}$ } =1040$ AU.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0890fig14.ps}\end{figure}$ Figure 13: TIMMI2 N-band spectrum of the UC H II region G268.42-0.85. The spectrum shows broad and deep silicate absorption feature with forbidden line emission from [Ar III] and [S IV]. The structures around 9.6 $\mu$ m and 11.3 $\mu$ m are probably artifacts, partly due to imperfect cancellation of the telluric ozone bands.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{0890fig15.ps}\end{figure}$ Figure 14: Spectral energy distribution of the G268.42-0.85 UC H II region. Crosses mark observations which were used for fitting the SED, squares denote data that are neglected in this regard (see Table 4). The source is modeled as a modified black body with 0.014 pc radius, 80 K temperature and a dust emissivity of $\epsilon _{\nu } \sim \nu ^{2.1 \pm 0.4}$ . Error bars are included according to the values given in Table 4 but remain tiny due to the logarithmic scaling of the plot.
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{0890fig16.ps}\end{figure}$ Figure 15: Simple sketch of the structure of the star-forming region IRAS 09002-4732. The likely relative line-of-sight positions are mainly deduced from the extinction pattern and different geometrical considerations as described in Sect. 4.1. The observer's direction is marked by an eye symbol.
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In the text

$\begin{figure} \par\includegraphics[width=13cm]{0890fig4.eps}\end{figure}$	Figure 3: False-colour composite image from the near-infrared observations. The Ks band image is coded in red, H in green and Js in blue.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0890fig5.ps}\end{figure}$	Figure 4: Js-band surface brightness of the reflection nebulosity versus the distance from the UC H II region G268.42-0.85 plotted on a logarithmic scale. The best fit gives an $R^{-1.4 \pm 0.2}$ dependence.
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$\begin{figure} \par\includegraphics[height=18.3cm,width=13cm]{0890fig6.eps} % \end{figure}$	Figure 5: Outlines of the filamentary structure of extincting material seen in the NIR images. The solid lines trace the general structure, while the dashed lines indicate the dark filaments (S1-S5). The dense globules inside the filaments are indicated with hatched ellipses and designated as G1-G15. The two circles (IS1 and IS2) mark two isolated silhouette objects.
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$\begin{figure} \par\includegraphics[height=7.1cm,width=7.1cm,clip]{0890fig7.ps}\end{figure}$	Figure 6: Unsharp-masked magnified field from Fig. 5 showing the objects IS1 and IS2.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0890fig8.eps}\end{figure}$	Figure 7: Ks-band inverted gray scale image. Crosses mark the 1106 stars identified in the Ks band, while boxes denoted those with identified infrared excess emission.
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$\begin{figure} \par\includegraphics[width=8.8cm]{0890fig10.ps}\end{figure}$	Figure 9: Near-infrared colour-magnitude diagram of the same stellar population as in Fig. 8. The symbols are identical to those used in Fig. 8. The assumed distance of the zero age main sequence stars is 1.3 kpc. Individual error bars are shown on each object, some of which are smaller than the actual symbols.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0890fig12.ps}\end{figure}$	Figure 11: Ks-band stellar density derived from stellar counts in concentric annuli around the UC H II region G268.42-0.85.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0890fig14.ps}\end{figure}$	Figure 13: TIMMI2 N-band spectrum of the UC H II region G268.42-0.85. The spectrum shows broad and deep silicate absorption feature with forbidden line emission from [Ar III] and [S IV]. The structures around 9.6 $\mu$ m and 11.3 $\mu$ m are probably artifacts, partly due to imperfect cancellation of the telluric ozone bands.
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$\begin{figure} \par\includegraphics[width=10.5cm,clip]{0890fig16.ps}\end{figure}$	Figure 15: Simple sketch of the structure of the star-forming region IRAS 09002-4732. The likely relative line-of-sight positions are mainly deduced from the extinction pattern and different geometrical considerations as described in Sect. 4.1. The observer's direction is marked by an eye symbol.
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