All Figures

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f1a.ps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{5731f1b.eps} \end{figure}$ Figure 1: The intensity map for the region around IRAS 14416-5937 at 150 $\mu$ m ( left) and 210 $\mu$ m ( right). Contour levels are at 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, and 95% of peak intensity of 2450 Jy/sq arcmin ( left) and 1367 Jy/sq arcmin ( right).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f2a.ps}\hspace*{4mm} \... ...f2c.ps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{5731f2d.ps} \end{figure}$ Figure 2: The IRAS-HIRES intensity map for the region covering IRAS 14416-5937 at 12 $\mu$ m ( top left), 25 $\mu$ m ( top right), 60 $\mu$ m ( bottom left), and 100 $\mu$ m ( bottom right). The contours are at 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, and 95% of the peak value of 155 Jy arcmin^-2, 1380 Jy arcmin^-2, 3360 Jy arcmin^-2, and 2410 Jy arcmin^-2 at 12, 25, 60, and 100 $\mu$ m, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f3a.ps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{5731f3b.ps} \end{figure}$ Figure 3: The distribution of dust temperature T(150/210) ( left), and optical depth at 200 $\mu$ m, $\tau _{200}$ , ( right) from the region around IRAS 14416-5937 assuming a dust emissivity law of $\epsilon _{\lambda } \propto \lambda ^{-2}$ . The isotherms correspond to 20, 25, 27, 32, 40, 50, and 60 K. The $\tau _{200}$ contours represent 5, 10, 20, 30, 40, 50, 60, 70, 80, and 90% of the peak value of 0.06.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f4.ps} \end{figure}$ Figure 4: The emission in UIBs for the region around IRAS 14416-5937. The contour levels are at 1, 5, 10, 20, 30, 40, 50, 60, 65, 70, 80, 90, and 95% of peak value of $1.3\times 10^{-4}$ W m^-2 Sr^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f5.ps} \end{figure}$ Figure 5: The SUMSS radio flux density map for the region around IRAS 14416-5937 at 843 MHz. The contour levels are at 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, and 95% of peak flux of 4.4 Jy/beam. The beam is $\sim$ $43\hbox {$^{\prime \prime }$ }\times 50\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f6.ps} \end{figure}$ Figure 6: ISO-LWS spectrum (solid line) shown along with the model calculations (dash-dotted line). The ISO-LWS spectrum is taken for a region $\sim$ 1.4' to the north-west of IRAS 14416-5937 - A. However, the model calculations are carried out for IRAS 14416-5937 - A.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f7a.ps}\hspace*{4mm} \includegraphics[width=5.7cm,clip]{5731f7b.ps} \end{figure}$ Figure 7: Colour-magnitude ( left) and colour-colour diagram ( right) for sources detected in all the three 2MASS bands for the region around IRAS 14416-5937. In the colour-magnitude diagram, the nearly vertical solid lines from left to right represent the zero age main sequence (ZAMS) curves reddened by A_V = 0, and 20 mag, respectively. The slanting lines trace the reddening vectors of these ZAMS stars. In the colour-colour diagram, the locii of the main sequence and giant branches are shown by the solid and dotted lines, respectively. The short-dash line represents the locus of T-Tauri stars. The three parallel dash-dotted straight lines follow the reddening vectors of giants, main sequence stars (or dwarfs), and the T-Tauri stars. The long dashed line represents the locus of Herbig Ae/Be stars. The asterisk symbols represent sources lying above the ZAMS curve B0. The open circles represent sources depicting an infrared excess in the colour-colour diagram. The dots are sources lying below the ZAMS spectral curve of B0 (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f8.ps} \end{figure}$ Figure 8: Colour-colour diagram of the sources detected in all the four bands of Spitzer-IRAC for the region around IRAS 14416-5937. The open circles, open squares, filled triangles, and cross symbols denote Class I, Class I/II, Class II, and other sources, respectively. The solid-line square in the diagram approximately delineates the region occupied by the Class II sources, whereas the dotted-line square covers the region occupied by the Class I sources as shown in the models of Allen et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f9a.ps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{5731f9b.ps} \end{figure}$ Figure 9: Comparison of the spectral energy distribution from observations and the best-fit radiative transfer model of IRAS 14416-5937 - A ( left) and IRAS 14416-5937 - B ( right). The open circles, triangles, and squares represent the TIFR, IRAS-HIRES and MSX data, respectively. The solid line is the best-fit radiative transfer model to the data. See text and Table 3 for details of the model parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5731f10.ps} \end{figure}$ Figure 10: Emergent spectrum from model calculations of IRAS 14416-5937 - A. Few lines are identified and the details of the lines are given Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f11.ps} \end{figure}$ Figure 11: The radio contours (SUMSS; 843 MHz) overlaid over the 2MASS $K_{\rm s}$ band image for the region around IRAS 14416-5937. The labelled axes are in J2000 coordinates. The regions "A'' and "B'' are shown and various near-infrared sources are marked. The asterisk symbols represent sources of spectral type earlier than B0, and the circles denote the infrared excess sources. The solid triangle represents J14452143-5949251 (2MASS source closest to radio peak detected in all the three ( $JHK_{\rm s}$ ) bands and of spectral type earlier than O6 from the CM diagram).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f12.ps} \end{figure}$ Figure 12: The spectral energy distribution of J14452143-5949251 (2MASS source closest to radio peak detected in all the three ( $JHK_{\rm s}$ ) bands and of spectral type earlier than O6 from the CM diagram) constructed using the fluxes from 2MASS and Spitzer-GLIMPSE (details in text).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f13.ps} \end{figure}$ Figure 13: Spitzer-GLIMPSE sources detected in all the four IRAC bands overlaid over the Spitzer-GLIMPSE 5.8 $\mu$ m band image for the region around IRAS 14416-5937. The labelled axes are in J2000 coordinates. The open circles, open squares, filled triangles, and cross symbols represent the Class I, Class I/II, Class II, and the other sources, respectively (see text for details). The sources "A'' and "B'' are marked. The OH, H₂O, and CH₃OH maser positions are shown by the light blue, yellow, and orange plus symbols, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f1a.ps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{5731f1b.eps} \end{figure}$	Figure 1: The intensity map for the region around IRAS 14416-5937 at 150 $\mu$ m ( left) and 210 $\mu$ m ( right). Contour levels are at 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, and 95% of peak intensity of 2450 Jy/sq arcmin ( left) and 1367 Jy/sq arcmin ( right).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f4.ps} \end{figure}$	Figure 4: The emission in UIBs for the region around IRAS 14416-5937. The contour levels are at 1, 5, 10, 20, 30, 40, 50, 60, 65, 70, 80, 90, and 95% of peak value of $1.3\times 10^{-4}$ W m^-2 Sr^-1.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f5.ps} \end{figure}$	Figure 5: The SUMSS radio flux density map for the region around IRAS 14416-5937 at 843 MHz. The contour levels are at 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, and 95% of peak flux of 4.4 Jy/beam. The beam is $\sim$ $43\hbox {$^{\prime \prime }$ }\times 50\hbox {$^{\prime \prime }$ }$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5731f6.ps} \end{figure}$	Figure 6: ISO-LWS spectrum (solid line) shown along with the model calculations (dash-dotted line). The ISO-LWS spectrum is taken for a region $\sim$ 1.4' to the north-west of IRAS 14416-5937 - A. However, the model calculations are carried out for IRAS 14416-5937 - A.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5731f10.ps} \end{figure}$	Figure 10: Emergent spectrum from model calculations of IRAS 14416-5937 - A. Few lines are identified and the details of the lines are given Table 4.
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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5731f12.ps} \end{figure}$	Figure 12: The spectral energy distribution of J14452143-5949251 (2MASS source closest to radio peak detected in all the three ( $JHK_{\rm s}$ ) bands and of spectral type earlier than O6 from the CM diagram) constructed using the fluxes from 2MASS and Spitzer-GLIMPSE (details in text).
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