All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fig1.ps} \end{figure}$ Figure 1: Observed spectra towards IC 10 nucleus (see Table B.1) except for the [CI](³P ₂-³P₁) and the ¹²CO(7-6) spectra which correspond to the offset position (0'', 30''). Velocities (horizontal axis) are given in km s^-1 relative to the LSR ( $V_{\rm LSR}$ ) and the line intensities (vertical axis) are in units of $T_{\rm mb}$ (K). The grey curves are Gaussian fits. The observed line is written above each spectrum. In this figure, we present the [CI](³P ₂-³P₁) and the ¹²CO(7-6) lines on the same spectrum since they have been observed simultaneously. The [CI](³P ₁-³P₀) spectrum is from Gerin & Phillips (2000) but it has been analyzed again to obtain an homogeneous dataset of observations.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig2.ps} \end{figure}$ Figure 2: Observed spectra towards IC 342 nucleus (see Table B.1). See the caption of Fig. 1. We present the [CI](³P ₂-³P₁) and the ¹²CO(7-6) lines on the same spectrum since they have been observed simultaneously.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig3.ps} \end{figure}$ Figure 3: Observed spectra towards M 82 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig6.ps} \end{figure}$ Figure 6: Observed spectra towards NGC 4038 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig7.ps} \end{figure}$ Figure 7: Observed spectra towards the Overlap region (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi12.ps} \end{figure}$ Figure 12: Observed spectra towards M 83 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi14.ps} \end{figure}$ Figure 14: Observed spectra towards NGC 6946 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3872fi17.ps} \end{figure}$ Figure 17: Map of the velocity integrated intensity of ¹²CO(3-2) ( top) and ¹²CO(6-5) ( bottom) towards IC 342. The CO emission is integrated over the velocity ranges -200 to 200 km s^-1 and -50 to 150 km s^-1, respectively. For both maps, the crosses show the observed positions. The contours of the ¹²CO(3-2) map range from $\int{T_{\rm mb}{\rm d}v} = 12$ K km s^-1 to 112 K km s^-1 with 10 K km s^-1 steps. For the ¹²CO(6-5) map, the contours range from $\int{T_{\rm mb}{\rm d}v} = 8$ K km s^-1 to 108 K km s^-1 with 10 K km s^-1 steps. The intensity peak value of the ¹²CO(3-2) map is $\int{T_{\rm mb}{\rm d}v} \approx 110$ K km s^-1. The intensity peak value of the ¹²CO(6-5) map is $\int{T_{\rm mb}{\rm d}v} \approx 108$ K km s^-1. The black box in the upper figure represents the size of the lower figure. The circles indicate the beam sizes at the frequency of the ¹²CO(3-2) line ( top) and at the frequency of the ¹²CO(6-5) line ( bottom). No pointing error was detected for this map.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi18.ps} \end{figure}$ Figure 18: Map of the velocity integrated intensity of ¹²CO(3-2) ( top) and ¹²CO(6-5) ( bottom) lines towards M 83. For both maps, the CO emission is integrated over the velocity range 200 to 800 km s^-1, and the crosses show the observed positions. The contours of the ¹²CO(3-2) map range from $\int{T_{\rm mb}{\rm d}v} = 3$ K km s^-1 to 18 K km s^-1 with 3 K km s^-1 steps, and from $\int{T_{\rm mb}{\rm d}v} = 21$ K km s^-1 to 102 K km s^-1 with 10 K km s^-1 steps. For the ¹²CO(6-5) map, the contours range from $\int{T_{\rm mb}{\rm d}v} = 20$ K km s^-1 to 320 K km s^-1 with 25 K km s^-1 steps. The intensity peak value of the ¹²CO(3-2) map is $\int{T_{\rm mb}{\rm d}v} \approx 100$ K km s^-1. The intensity peak value of the ¹²CO(6-5) map is $\int{T_{\rm mb}{\rm d}v} \approx 318$ K km s^-1. The ¹²CO(6-5) map has been shifted by +5'' along the minor axis due to a pointing error The black box in the upper figure represents the size of the lower figure. The circles indicate the beam size at the frequency of the ¹²CO(3-2) line ( top) and at the frequency of the ¹²CO(6-5) line ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=12.65cm,clip]{3872fi19.ps} \end{figure}$ Figure 19: LVG model results for NGC 4038 ( right side) and M 83 ( left side). For each source, the "best'' fit N(¹²CO)/ $\Delta v$ (indicated at the top) is found by minimizing $\chi ^{2}$ . In fact, to avoid gridding problems, we use all models within a small interval centered around the best N(¹²CO)/ $\Delta v$ value, listed in Table 3. We plot $\Delta \chi ^{2}$ contours in the T_K (K) vs. n(H₂)(cm^-3) space. The contour levels for M 83 and for NGC 4038 are indicated in the plots. The LVG models with higher $\Delta \chi ^{2}$ (>4) are not represented. In both figures, the dark areas represent the zones where $\chi ^{2}$ is the lowest. Each cross corresponds to a LVG model solution. The best fit is located at the intersection of the two black lines.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3872fi20.ps} \end{figure}$ Figure 20: ``best'' LVG and PDR models compared with observations for IC 10 (see Table 3 for the model parameters). On the left side, we plot integrated intensities in K km s^-1 vs. $J_{\rm upper}$ . On the right side, we plot I in Wm^-2 sr^-1 vs. $J_{\rm upper}$ . In all figures, grey triangles represent the LVG model while the grey squares represent results from the PDR model (see Sect. 5.3). Observations (with error bars) taken from the literature and from our data set are shown in black. The ¹³CO transitions are represented with open symbols while the ¹²CO transitions use filled symbols.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3872fi21.ps} \end{figure}$ Figure 21: "best''LVG and PDR models compared with observations for IC 342 (see Table 3 for the model parameters). See caption of Fig. 20.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi22.ps} \end{figure}$ Figure 22: "best'' LVG and PDR models compared with observations for NGC 4038 (see Table 3 for the model parameters). See caption of Fig. 20.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi23.ps} \end{figure}$ Figure 23: "best'' LVG and PDR models compared with observations for Overlap (see Table 3 for the model parameters). See caption of Fig. 20.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi24.ps} \end{figure}$ Figure 24: "best'' LVG and PDR models compared with observations for M 83 (see Table 3 for the model parameters). See caption of Fig. 20.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi25.ps} \end{figure}$ Figure 25: "best'' LVG and PDR models compared with observations for NGC 6946 (see Table 3 for the model parameters). See caption of Fig. 20.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi26.ps} \end{figure}$ Figure 26: Flux (Wm^-2) vs. $J_{\rm upper}$ for the center of the Milky Way ( top left, triangles), IC 342 ( top left, points), NGC 6946 ( top right, points), M 83 ( top right, triangles), the Cloverleaf QSO ( bottom left, triangles), Henize 2-10 ( bottom left, points) IC 10 ( bottom right, triangles) and NGC 253 ( bottom right, points). PDR models (grey points or grey triangles) have been used to obtained line fluxes of unobserved lines (e.g. ¹²CO(5-4), ¹²CO(7-6), ¹²CO(8-7), ¹²CO(9-8), ...) depending on the completeness of the dataset obtained for each source. Observations are shown in black with error bars. To ease the comparison, we applied scaling factors on all sources data except for NGC 253. The value of these scaling factors is specified for each source on the plots. We notice that for the Cloverleaf QSO, the ¹²CO(1-0) line flux is an upper limit (see Tsuboi et al. 1999).
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{3872fi27.ps} \end{figure}$ Figure 27: Flux (Wm^-2) vs. $J_{\rm upper}$ for the NGC 4038 nucleus (points). See the caption of Fig. 26. In this figure, we plot observations of the ¹²CO(4-3) and ¹²CO(7-6) lines even though they have a low signal-to-noise ratio. We also plot their PDR predicted fluxes.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig4.ps} \end{figure}$ Figure 4: Observed spectra towards NGC 3079 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig5.ps} \end{figure}$ Figure 5: Observed spectra towards IRAS 10565+2448 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig8.ps} \end{figure}$ Figure 8: Observed spectra towards NGC 4736 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig9.ps} \end{figure}$ Figure 9: Observed spectra towards Markarian 231 nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fi10.ps} \end{figure}$ Figure 10: Observed spectra towards Centaurus A nucleus (see Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi11.ps} \end{figure}$ Figure 11: Spectra of M 51 at various offset positions relative to the central position (0'', 0'',) given in Table 1 (see also Table B.1) : (-24'', -24'') ( top), (0'', 0'') ( middle) and (0'', 12'') ( bottom). See the caption of Fig. 1. The [CI](³P ₁-³P₀) spectrum at the central position (0'', 0'') is from Gerin & Phillips (2000) but it has been analyzed again to obtain an homogeneous dataset of observations.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fi13.ps} \end{figure}$ Figure 13: Observed spectra towards Arp 220 nucleus (see Table B.1). See the caption of Fig. 1. In this figure, both spectra are from Gerin & Phillips (1998) but they have been analyzed again to obtain an homogeneous dataset of observations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi15.ps} \end{figure}$ Figure 15: Spectra taken in the M 83 arms at the offset positions ( 90''-100'', 30'') ( top) and (-90'', -60'') ( bottom) (relative to the central position (0'', 0'') listed in Table 1, see also Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi16.ps} \end{figure}$ Figure 16: Spectra taken towards the NGC 6946 arms at the offset positions (110'', 100'') ( top) and (150'', -20'') ( bottom) (relative to the central position (0'', 0'') listed in Table 1, see also Table B.1). See the caption of Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig2.ps} \end{figure}$	Figure 2: Observed spectra towards IC 342 nucleus (see Table B.1). See the caption of Fig. 1. We present the [CI](³P ₂-³P₁) and the ¹²CO(7-6) lines on the same spectrum since they have been observed simultaneously.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig3.ps} \end{figure}$	Figure 3: Observed spectra towards M 82 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig6.ps} \end{figure}$	Figure 6: Observed spectra towards NGC 4038 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3872fig7.ps} \end{figure}$	Figure 7: Observed spectra towards the Overlap region (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi12.ps} \end{figure}$	Figure 12: Observed spectra towards M 83 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi14.ps} \end{figure}$	Figure 14: Observed spectra towards NGC 6946 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3872fi21.ps} \end{figure}$	Figure 21: "best''LVG and PDR models compared with observations for IC 342 (see Table 3 for the model parameters). See caption of Fig. 20.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi22.ps} \end{figure}$	Figure 22: "best'' LVG and PDR models compared with observations for NGC 4038 (see Table 3 for the model parameters). See caption of Fig. 20.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi23.ps} \end{figure}$	Figure 23: "best'' LVG and PDR models compared with observations for Overlap (see Table 3 for the model parameters). See caption of Fig. 20.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi24.ps} \end{figure}$	Figure 24: "best'' LVG and PDR models compared with observations for M 83 (see Table 3 for the model parameters). See caption of Fig. 20.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{3872fi25.ps} \end{figure}$	Figure 25: "best'' LVG and PDR models compared with observations for NGC 6946 (see Table 3 for the model parameters). See caption of Fig. 20.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{3872fi27.ps} \end{figure}$	Figure 27: Flux (Wm^-2) vs. $J_{\rm upper}$ for the NGC 4038 nucleus (points). See the caption of Fig. 26. In this figure, we plot observations of the ¹²CO(4-3) and ¹²CO(7-6) lines even though they have a low signal-to-noise ratio. We also plot their PDR predicted fluxes.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig4.ps} \end{figure}$	Figure 4: Observed spectra towards NGC 3079 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig5.ps} \end{figure}$	Figure 5: Observed spectra towards IRAS 10565+2448 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig8.ps} \end{figure}$	Figure 8: Observed spectra towards NGC 4736 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fig9.ps} \end{figure}$	Figure 9: Observed spectra towards Markarian 231 nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fi10.ps} \end{figure}$	Figure 10: Observed spectra towards Centaurus A nucleus (see Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3872fi13.ps} \end{figure}$	Figure 13: Observed spectra towards Arp 220 nucleus (see Table B.1). See the caption of Fig. 1. In this figure, both spectra are from Gerin & Phillips (1998) but they have been analyzed again to obtain an homogeneous dataset of observations.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi15.ps} \end{figure}$	Figure 15: Spectra taken in the M 83 arms at the offset positions ( 90''-100'', 30'') ( top) and (-90'', -60'') ( bottom) (relative to the central position (0'', 0'') listed in Table 1, see also Table B.1). See the caption of Fig. 1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3872fi16.ps} \end{figure}$	Figure 16: Spectra taken towards the NGC 6946 arms at the offset positions (110'', 100'') ( top) and (150'', -20'') ( bottom) (relative to the central position (0'', 0'') listed in Table 1, see also Table B.1). See the caption of Fig. 1.
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