All Figures

$\begin{figure} \par\mbox{ \includegraphics[width=8.7cm,clip]{0336fg1.eps} \hspace*{4mm} \includegraphics[width=8.7cm,clip]{0336fg2.eps} } \end{figure}$ Figure 1: ( Left) Las Campanas color composite image of IRAS 19410+2336 where J is blue, H is green and $K_{\rm s}$ is red. Stars which are discussed in the text are labeled. ( Right) In grey-scale we show the broad-band ( $K_{\rm s}$ filter) acquisition image of IRAS 19410+2336 obtained with LIRIS. A dotted box outlines the field-of-view covered by the Las Campanas $JHK_{\rm s}$ data. The black small circles indicate the positions of the H₂ knots 1 and 2 detected in one of the two LIRIS slits (slit #1). The large dashed circles mark the positions and approximate sizes of the two massive star-forming clumps detected at 1.2 mm with the IRAM 30 m telescope. The white contours outline the Spitzer 5.8 $\mu$ m emission (more detailed MIR images of the central source are shown in Fig. 2). The red asterisks mark the positions of the mm sources identified by Beuther et al. (2003). The orange filled triangle marks the position of the cm continuum source associated with H₂O and CH₃OH maser emission (Beuther et al. 2002d). Blue squares mark the X-ray sources observed by Beuther et al. (2002a). The green stars are 2MASS point sources of interest. The (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) position in both images corresponds to RA (J2000.0 $)=19^{\rm h}$ 43 $^{\rm m}$ 11 $.\!\!^{\rm s}$ 18 and Dec (J2000.0 $)=23\degr44\hbox{$^\prime$ }04\hbox{$.\!\!^{\prime\prime}$ }2$ (see the electronic edition of the Journal for a color version of this figure).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.7cm,clip]{0336fg3.eps} \hspace*{4mm} \includegraphics[width=8.7cm,clip]{0336fg4.eps} } \end{figure}$ Figure 2: Spitzer/IRAC 3.6 and 5.8 $\mu$ m images of the central part of IRAS 19410+2336. White contours represent the $K_{\rm s}$ emission. The mm sources identified by Beuther et al. (2003) are indicated by asterisks. The triangle marks the position of the cm continuum source. In these figures, north is up and east is to the left. The (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) position corresponds to RA (J2000.0 $)=19^{\rm h}$ 43 $^{\rm m}$ 11 $.\!\!^{\rm s}$ 18 and Dec (J2000.0) = 23$^$44 $^\prime$ 04 $.\!\!^{\prime\prime}$ 2 (see the electronic edition of the Journal for a color version of this figure).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0336fg5.eps} \end{figure}$ Figure 3: Contours of the broad-band ( $K_{\rm s}$ filter) acquisition image of IRAS 19410+2336 obtained with LIRIS. The positions of the slits and the distinct regions analysed in the text are marked. Regions 3 and 4, which correspond respectively to H₂ knots 1 and 2 (see the right panel of Fig. 1), are 50 $^{\prime \prime }$ and 119 $^{\prime \prime }$ north of nr56. The red stars indicate, from right to left, the positions of sources nr56, nr56b, nr56c and nr56d. In this figure, north is up and east is to the left. The (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) position corresponds to RA (J2000.0 $)=19^{\rm h}$ 43 $^{\rm m}$ 11 $.\!\!^{\rm s}$ 18 and Dec (J2000.0) = 23$^$44 $^\prime$ 04 $.\!\!^{\prime\prime}$ 2 (see the electronic edition of the Journal for a color version of this figure).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.4cm,clip]{0336fg6.eps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{0336fg7.eps} } \end{figure}$ Figure 4: ( Left) NIR color-color diagram of IRAS 19410+2336. The solid line represents the main sequence from Tokunaga (2000) and Martins & Plez (2006). The dashed lines show the reddening band for main sequence colors. A reddening vector of 2 mag in the K-band is represented by a thick arrow. Blue squares indicate sources associated with X-ray emission. Orange diamonds are objects which are associated with strong MIR emission. Finally, various 2MASS point sources of interest are plotted by green stars. We include 2MASS_4, the 2MASS point source associated with the H₂ knot 2. ( Right) NIR color-magnitude diagram at a distance of 2.1 kpc. Here, the dashed lines show our detection limits, and the dotted lines comprise the area where reddened O and early B stars at a distance of 2.1 kpc might be found (see the electronic edition of the Journal for a color version of this figure).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0336fg8.eps} \end{figure}$ Figure 5: Spitzer/IRAC color-color diagram for sources with identifications in all four IRAC bands. The thick vector on the left shows A_K=2. We use the same symbols here as in Fig. 4. The dashed lines and labels for different types of protostars are based on the classification of Megeath et al. (2004) (see the electronic edition of the Journal for a color version of this figure).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0336fg9.eps} \end{figure}$ Figure 6: Spatial variation of the H₂ 1-0 S(1) transition at 2.121 $\mu$ m across slits #1 and #2. The origin corresponds to the (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) position of Fig. 3. The different regions analysed in the text (1 to 9) are identified. Regions 3 and 4 correspond to H₂ knots 1 and 2, respectively. The stars indicate the positions of sources nr56, nr56b, nr56c and nr56d.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.5cm,clip]{0336fg10.eps} \hspace*{4mm} \includegraphics[width=8.1cm,clip]{0336fg11.eps} } \end{figure}$ Figure 7: ( Left) Spectra of various regions along slit #1 ( $\rm PA= 0\hbox {$^\circ $ }$ ). The lower panel shows the integrated spectra across slit #2 ( $\rm PA=59\hbox {$^\circ $ }$ ). The positions of the strongest H₂ lines and Br $\gamma$ are indicated by dotted lines. ( Right) Spectra of sources nr56, nr56b, nr56c and nr56d. The positions of Br $\gamma$ and the CO bandheads are marked. These four spectra have been corrected for extinction using the values listed in Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{0336fg12.eps} \end{figure}$ Figure 8: H₂ excitation diagrams for every region (except region 2, where only two useful lines are available). The lines represent the best fitting purely thermal single-temperature models.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0336fg13.eps} \end{figure}$ Figure 9: Spatial variation across slit #2 ( $\rm PA=59\hbox {$^\circ $ }$ ) of the ortho-to-para ratio ( $\phi _1$ ), the extinction ( $A_{\rm K}$ ) and the excitation temperature ( $T_{\rm ex}$ ). In grey we show the average results from the integrated spectrum across this slit. Offsets are the same as in the top panel of Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0336fg8.eps} \end{figure}$	Figure 5: Spitzer/IRAC color-color diagram for sources with identifications in all four IRAC bands. The thick vector on the left shows A_K=2. We use the same symbols here as in Fig. 4. The dashed lines and labels for different types of protostars are based on the classification of Megeath et al. (2004) (see the electronic edition of the Journal for a color version of this figure).
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{0336fg12.eps} \end{figure}$	Figure 8: H₂ excitation diagrams for every region (except region 2, where only two useful lines are available). The lines represent the best fitting purely thermal single-temperature models.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0336fg13.eps} \end{figure}$	Figure 9: Spatial variation across slit #2 ( $\rm PA=59\hbox {$^\circ $ }$ ) of the ortho-to-para ratio ( $\phi _1$ ), the extinction ( $A_{\rm K}$ ) and the excitation temperature ( $T_{\rm ex}$ ). In grey we show the average results from the integrated spectrum across this slit. Offsets are the same as in the top panel of Fig. 6.
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