All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{brooks_fig1.eps}\end{figure}$ Figure 1: A contour representation of IRAS 60 $\mu$ m emission superimposed on an H $\alpha$ image taken from the Digitized Sky Survey. Contour levels range from 10 to 99% of the peak emission of 29 500 MJy sr^-1 in increments of 8%. The regions bounded by the respective thick dashed and solid lines indicate the extent of the [C II] 158 $\mu$ m and $\rm ^{13}CO(2{-}1)$ data discussed in this work. The thin dashed line marks the cut (joining Tr 14 to the far-infrared peak emission) used for the set of intensity-position diagrams shown in Fig. 11 and the five squares mark the positions along the central raster for the ISO observations. The centers of Tr 14 and Tr 16 (denoted by the star $\eta$ Car) are also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{brooks_fig2.eps}\end{figure}$ Figure 2: Maps of a) [C II] 158 $\mu$ m emission and b) [O I] 63 $\rm\mu m$ emission. The contour levels are 0.35 ( $3\sigma$ ), 0.50, 0.65, 0.80, 0.95, 1.10, 1.25, 1.40, $\rm 1.56 \times 10^{-3} ~ erg s^{-1} ~ cm^{-2} ~ sr^{-1}$ for the [C II] map, and 3.1, 3.6, 4.2, 4.8, 5.5 $\rm 5.9 \times 10^{-3} ~ erg ~ s^{-1} ~ cm^{-2} ~sr^{-1}$ for the [O I] map. The grid of dots represent the observed positions. Their offsets are given with respect to the position RA(J2000) = $10^{\rm h}43^{\rm m}26.1^{\rm s}$ , Dec(J2000) = $-59^{\circ }35\hbox {$^\prime $ }45\hbox {$^{\prime \prime }$ }$ . The center of Tr 14 is marked by the cross.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{brooks_fig3.eps}\end{figure}$ Figure 3: LWS spectra (solid line) at three positions across the Tr 14 region, corresponding to the H II region (-200 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ), the far-infrared peak (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) and the molecular cloud (+200 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ). The best-fitted modified blackbody spectra (dashed line) are shown (see text) and the fine-structure lines are identified.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{brooks_fig4.eps}\end{figure}$ Figure 4: Variation of the intensity of the fine-structure lines and the dust temperature across the Tr 14 region taken from the ISO LWS observations. The location of the five data points are marked in Fig. 1 and their offsets are given with respect to the peak position (RA(J2000) = $\rm 10^{h}43^{m}20^{s}$ , Dec(J2000) = $-59^{\circ }34\hbox {$^\prime $ }28.4\hbox {$^{\prime \prime }$ }$ ) along the east-west direction. a) The [C II] 158 $\rm\mu m$ line and the two [O I] lines at 63 and 145 $\rm\mu m$ (dashed and dotted lines, respectively). b) The distributions of the [O III] 88 $\rm\mu m$ line (dotted) and the dust temperature (dashed).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{brooks_fig5.eps}\end{figure}$ Figure 5: Maps of ¹³CO, CO and CS emission integrated over the velocity range -35 to -5 km s^-1. The grid of dots show the observed positions, where the offsets are with respect to the reference position used in Fig. 2. The dashed box in the ¹³CO(2-1) map delineates the region which was subsequently mapped in ¹²CO(2-1) and CS(3-2). a) ¹³CO(2-1) emission with contour levels 20 (3 $\sigma$ ), 30, 40, 50, 60, 70, 80, 90, 100, 110, 120 K km s^-1. b) ¹²CO(2-1) emission with contours from 20 to 80% of the peak emission 449 K km s^-1 in increments of 10%. c) CS(3-2) emission with contours from 20 to 90% of the peak emission 14 K km s^-1 in increments of 10%.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=18cm,clip]{brooks_fig6.eps}\end{figure}$ Figure 6: ¹²CO(2-1) (solid line) and ¹³CO(2-1) (dashed line) spectra. The offset positions indicated in each box (in arcsec) are given with respect to the reference position used in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{brooks_fig7.eps}\end{figure}$ Figure 7: Channel maps of the ¹³CO(2-1) emission integrated over 4 velocity ranges indicated in the upper left corners of each panel. The contour levels are 3 (3 $\sigma$ ), 9, 15, 21, 27, 33, 39, 45, 51 K km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{brooks_fig8.eps}\end{figure}$ Figure 8: CS(5-4), (3-2) and (2-1) spectra averaged over the whole map. The four main velocity intervals determined by the CO observations are indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{brooks_fig9.eps}\end{figure}$ Figure 9: LTE clump-mass distribution for 282 clumps found by the clump-finding algorithm GAUSSCLUMPS. N is the number of clumps in each mass bin.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{brooks_fig10.eps}\end{figure}$ Figure 10: Comparison of different emission tracers in the Tr 14 region. a) MSX $8~\mu$ m emission with contours of the 4.8-GHz radio continuum emission taken from Brooks et al. (2001). The contour levels are 0.08, 0.15, 0.2, 0.25, 0.3, 0.35, 0.4, 0.45, 0.5, 0.55, 0.6, 0.65 Jy beam^-1. b) MSX $20~\mu$ m emission with contours of the KAO [C II] $158~\mu$ m emission taken from Fig. 2. c) ¹³CO(2-1) emission taken from Fig. 5 with contours of the KAO [C II] $158~\mu$ m emission.The center of Tr 14 is marked by the cross.
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In the text

$\begin{figure} \par\includegraphics[width=16.6cm,clip]{brooks_fig11.eps}\end{figure}$ Figure 11: Emission brightness as a function of position along the cut shown in Fig. 1. The position units are in arcmin (1 arcmin = 0.65 pc at a distance of 2.2 kpc) with respect to the center of Tr 14. [C I] 492 GHz data has been taken from Zhang et al. (2000), 4.8-GHz data from Brooks et al. (2001) and PAH 3.29 $\mu$ m data from Rathborne et al. (2002). Note the PAH 3.29 $\mu$ m data contains stellar (continuum) emission. The dashed vertical line marks the boundary of the dust lane.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{brooks_fig12.eps}\end{figure}$ Figure 12: Schematic representation of the Tr 14 region based on the data discussed in this paper.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=18cm,clip]{brooks_fig6.eps}\end{figure}$	Figure 6: ¹²CO(2-1) (solid line) and ¹³CO(2-1) (dashed line) spectra. The offset positions indicated in each box (in arcsec) are given with respect to the reference position used in Fig. 2.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{brooks_fig7.eps}\end{figure}$	Figure 7: Channel maps of the ¹³CO(2-1) emission integrated over 4 velocity ranges indicated in the upper left corners of each panel. The contour levels are 3 (3 $\sigma$ ), 9, 15, 21, 27, 33, 39, 45, 51 K km s^-1.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{brooks_fig8.eps}\end{figure}$	Figure 8: CS(5-4), (3-2) and (2-1) spectra averaged over the whole map. The four main velocity intervals determined by the CO observations are indicated.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{brooks_fig9.eps}\end{figure}$	Figure 9: LTE clump-mass distribution for 282 clumps found by the clump-finding algorithm GAUSSCLUMPS. N is the number of clumps in each mass bin.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{brooks_fig12.eps}\end{figure}$	Figure 12: Schematic representation of the Tr 14 region based on the data discussed in this paper.
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