Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{3187f1.eps} \end{figure}$ Figure 1: The [C II] emission distribution as grey scale (with contour levels from (0.5 to 8.5 by 1) $\times$ 10^-4 erg sr^-1 s^-1 cm^-2) shows a pronounced peak close to the position of the exciting star S 106 IR (marked by a star symbol). The two squares denote the locations of peak dust continuum emission at 1.3 mm (Mezger et al. 1987) and at 450 $\mu$ m and 800 $\mu$ m (Richer et al. 1993). The western peak is referred to as S 106 FIR. Overlaid as white contours is the [O I] 63 $\mu$ m map (the square box indicates the mapped region) with contour levels from (2.3 to 20.7 by 2.3) $\times$ 10^-3 erg sr^-1 s^-1 cm^-2 increasing from outside to inside.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.3cm]{3187f2.eps} \end{figure}$ Figure 2: Spectra of [C I] 2 $\to$ 1 (grey shaded, spectra are smoothed to 1.6 km s^-1 resolution) and [C I] 1 $\to$ 0 (black line) emission, overlaid on an IR image of Subaru (each spectrum is centered on the appropriate position, e.g., the lower left box shows the spectrum taken towards the position 110'', -110''). The grey contours (levels 0.85 to 13.6 by 0.85 K km s^-1) represent the -1.3 km s^-1 velocity plane of ¹³CO 2 $\to$ 1 emission obtained with IRAM (Schneider et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3187f3.eps}\par\vspace*{2mm} \includegraphics[width=15.5cm,clip]{3187f4.eps} \end{figure}$ Figure 3: Maps of the line integrated [C I] 1 $\to$ 0 (top) and 2 $\to$ 1 (bottom) emission in the velocity range -7 to 7 km s^-1. The contour ranges are as follows (in the notation start/end/step): [C I] 1 $\to$ 0: 4/28/4 K km s^-1 (3 $\sigma =3.6$ K km s^-1), [C I] 2 $\to$ 1: 24/62/9.5 K km s^-1 (3 $\sigma =12$ K km s^-1). S 106 IR is marked by a star, the triangle indicates the position close to the NH₃ emission peak where an ISO LWS scan was taken.
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3187f5.eps} \end{figure}$ Figure 4: ISO LWS grating for S 106 IR (top line) and S 106 West (bottom line). The high-J CO lines and FIR PDR tracing lines are marked.
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In the text

$\begin{figure} \par\includegraphics[height=160mm,angle=-90,clip]{3187f6.eps}\par\vspace*{2mm} \includegraphics[height=90mm,angle=0,clip]{3187f7.eps} \end{figure}$ Figure 5: Maps of the line integrated CO 4 $\to$ 3 (top) and CO 7 $\to$ 6 (bottom) emission in the velocity range -7 to 7 km s^-1. The contour ranges are as follows (in the notation start/end/step): CO 4 $\to$ 3: 15/180/15 K km s^-1 (3 $\sigma =12$ K km s^-1), CO 7 $\to$ 6: 27/287/20 K km s^-1 (3 $\sigma =13.5$ K km s^-1). S 106 IR is marked by a star, the triangle indicates the position close to the NH₃ emission peak where an ISO LWS scan was taken.
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In the text

$\begin{figure} \par\includegraphics[width=12.6cm,angle=-90,clip]{3187f8.eps} \end{figure}$ Figure 6: Spectra of ¹²CO 7 $\to$ 6 emission (smoothed to a velocity resolution of 1.2 km s^-1) plotted on an IR picture of S 106 made with Subaru. The grey contours (levels 1 to 7 by 1 K km s^-1) represent the 2.5 km s^-1 velocity plane of ¹³CO 2 $\to$ 1 emission obtained with IRAM (Schneider et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{3187f9.eps} \end{figure}$ Figure 7: Left top and bottom: grey scale maps of the line integrated CN 3 $\to$ 2 and CS 7 $\to$ 6 emission both at 14'' angular resolution. Right top and bottom: the same molecular line maps as contours, overlaid on the [O I] 63 $\mu$ m emission at 22'' resolution as a grey scale. Both lines are integrated over a velocity range of -7 to 1 km s^-1. Contours start at the 3 $\sigma$ -level of 1.95 K km s^-1 and increase in steps of 3 $\sigma$ . The position of S 106 IR is marked by a star, the Mezger et al. (1987) submm peaks by squares and the source S 106 FIR as a rhombus.
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In the text

$\begin{figure} \par\includegraphics[height=130mm,angle=-90,clip]{3187f10.eps} \end{figure}$ Figure 8: Maps of the line integrated [C I] 1 $\to$ 0 emission (as a grey scale) overlayed with ¹³CO 2 $\to$ 1 emission as white contours. The position of S 106 IR is marked by a star and the ISO LWS position as a triangle. The contour ranges are (in the notation start/end/step): ¹³CO 2 $\to$ 1 40/160/20 K km s^-1(3 $\sigma =23.5$ K km s^-1), and [C I] 1 $\to$ 0 4/28/4 K km s^-1(3 $\sigma =3.6$ K km s^-1).
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In the text

$\begin{figure} \par\includegraphics[height=98mm,angle=-90,clip]{3187f11.eps}\par... ...ace*{2mm} \includegraphics[height=95mm,angle=-90,clip]{3187f13.eps} \end{figure}$ Figure 9: Maps of the line integrated CO 7 $\to$ 6 emission (as a grey scale) overlayed with ¹²CO 2 $\to$ 1 a), [C II] 158 $\mu$ m b), [C I] 2 $\to$ 1 c) emission as white/dashed contours. The positions of S 106 IR is marked as a star and the ISO LWS position as a triangle. The contour ranges are (in the notation start/end/step): ¹²CO 2 $\to$ 1 60/540/40 K km s^-1, [C II] 0.46/7.82/0.92 erg s^-1 sr^-1 cm^-2 (2 $\sigma =0.92$ erg s^-1 sr^-1 cm^-2), [C I] 2 $\to$ 1 are 24/62/9.5 K km s^-1 (3 $\sigma =12$ K km s^-1), and CO 7 $\to$ 6 40/280/40 K km s^-1 (3 $\sigma =13.5$ K km s^-1).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3187f14.eps} \end{figure}$ Figure 10: Linear correlation of the integrated intensity of [C I] 1 $\to$ 0 with ¹³CO 1 $\to$ 0 (filled circles) and ¹³CO 2 $\to$ 1 (open circles) at each position in S 106. The dashed lines show the least-squares fits to the data. The error bars indicate an assumed 20%(10%) uncertainty on the [C I] (¹³CO) line integrated intensity.
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In the text

$\begin{figure} \par\includegraphics[width=110mm,angle=0,clip]{3187f15.eps} \end{figure}$ Figure 11: The top panel a) shows the normalized line integrated intensities (in [erg s-1 sr^-2 cm^-2]) of [C II] 158 $\mu$ m, [C I] 2 $\to$ 1 and 1 $\to$ 0, and ¹²CO 7 $\to$ 6, 4 $\to$ 3, and CO 2 $\to$ 1 (all at 55'' resolution) along an east-west cut at the Declination of the star S 106 IR. The typical errors of the intensities are around 5% for the [C II] and low-J CO lines, and around 15%-20% for the [C I] and medium-J CO lines. The following panels display excitation temperatures b), integrated line intensity ratios with the intensities in K kms^-1 c), column density ratios d), and column densities e). The line ratio [C I] 2 $\to$ 1/1 $\to$ 0 is displayed a factor of 2 weaker and $T_{\rm ex}$ derived from this ratio a factor of 5 weaker than the actual values.
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In the text

$\begin{figure} \par\includegraphics[width=65mm,angle=0,clip]{3187f16.eps}\hspace*{3mm} \includegraphics[width=62mm,angle=0,clip]{3187f17.eps} \end{figure}$ Figure 12: Various FIR- and Submm molecular and atomic line ratios observed at S 106 IR ( left) and S 106 W (-120'', 0) ( right) are displayed within a parameter space for density and UV flux based upon a PDR-model from Kaufman et al. (1999). The plot for S 106 W shows as a grey scale the distribution of the reduced $\chi ^2$ . The contour level indicates the 1 $\sigma$ standard deviation of the minimum $\chi ^2$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3187f18.eps} \end{figure}$ Figure 13: The UV flux ( top) and particle density ( bottom) along the cut obtained by comparing the observed data with the PDR model of Kaufman et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3187f5.eps} \end{figure}$	Figure 4: ISO LWS grating for S 106 IR (top line) and S 106 West (bottom line). The high-J CO lines and FIR PDR tracing lines are marked.
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$\begin{figure} \par\includegraphics[width=12.6cm,angle=-90,clip]{3187f8.eps} \end{figure}$	Figure 6: Spectra of ¹²CO 7 $\to$ 6 emission (smoothed to a velocity resolution of 1.2 km s^-1) plotted on an IR picture of S 106 made with Subaru. The grey contours (levels 1 to 7 by 1 K km s^-1) represent the 2.5 km s^-1 velocity plane of ¹³CO 2 $\to$ 1 emission obtained with IRAM (Schneider et al. 2002).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3187f14.eps} \end{figure}$	Figure 10: Linear correlation of the integrated intensity of [C I] 1 $\to$ 0 with ¹³CO 1 $\to$ 0 (filled circles) and ¹³CO 2 $\to$ 1 (open circles) at each position in S 106. The dashed lines show the least-squares fits to the data. The error bars indicate an assumed 20%(10%) uncertainty on the [C I] (¹³CO) line integrated intensity.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3187f18.eps} \end{figure}$	Figure 13: The UV flux ( top) and particle density ( bottom) along the cut obtained by comparing the observed data with the PDR model of Kaufman et al. (1999).
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