Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[height=8.4cm,clip]{0469fig1.eps} } \end{figure}$ Figure 1: SCUBA calibrated and background-corrected 850 $\mu$ m grey-scale image of M 51 with 850 $\mu$ m contour superimposed. The contour levels are 13.5 (=1.6 $\sigma$ ), 27, 40.5, 58.5, 72, 90 and 117 mJy/beam. 13.5 mJy/beam corresponds to 2.6 MJy sr^-1. This image clearly shows the extended 850 $\mu$ m disk. The small source to the north is the nucleus of NGC 5195.
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In the text

$\begin{figure} \par {\includegraphics[height=8.4cm,clip]{0469fig2.eps} } {\includegraphics[height=8.4cm,clip]{0469fig3.eps} } \end{figure}$ Figure 2: Top: fitted exponential disk subtracted from the total 850 $\mu$ m emission as shown in Fig. 1. Contour steps are 6 mJy/beam (1.15 MJy sr^-1). The maximum intensity of the disk is 66 mJy/beam with a major axis scale-length of 1.95 $^{\prime }$ . Bottom: contours of 850 $\mu$ m in M 51 after subtraction of the exponential disk superimposed on a 6400 Å optical image (Tilanus et al. 1988). Contour levels are 12 (=1.5 $\sigma$ ; 2.3 MJy sr^-1), 24, 36, 56 and 72 mJy/beam. The image shows the centroid of the 850 $\mu$ m emission to be located along the inner edges of the spiral arms and the optical dust lanes.
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In the text

$\begin{figure} \par {\includegraphics[width=8.4cm,clip]{0469fig4.ps} } \end{figure}$ Figure 3: The model exponential disk (crosses) compared to the actual emission of the M 51 disk (solid line), for $h_{\rm d}=7.65$ kpc, $h_{\rm s}=3.15$ kpc, $L=1.1\times 10^{11}\ L_\odot$ , $\tau _{V,f}=4.35$ and no CO contamination.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0469fig5.ps} } \end{figure}$ Figure 4: Resulting optical depth for different luminosities assuming either zero CO contamination ( upper line) or an omnipresent maximum 12 per cent contamination ( lower line). The shaded area shows the possible solutions.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm, clip]{0469fig6.ps} } \end{figure}$ Figure 5: Radial temperature profile for a total luminosity for M 51 of $L=1.1\times 10^{11}~L_\odot$ . The solid line marks zero CO contamination, the dotted line a maximum 12 per cent contamination, and the dashed line a contamination decreasing from maximum in the center to zero at the outer edge of M 51.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm, clip]{0469fig7.ps} } \end{figure}$ Figure 6: The dust surface density profiles for a graphite and silicate ratio of 0.5:0.5 and $\kappa_{850} = 1.2~\rm g^{-1}~\rm cm^{2}$ ; no CO contribution (solid line), 12 percent CO contribution (dotted line) and decreasing CO contribution (dashed line).
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In the text

$\begin{figure} \par {\includegraphics[height=8.4cm,clip]{0469fig1.eps} } \end{figure}$	Figure 1: SCUBA calibrated and background-corrected 850 $\mu$ m grey-scale image of M 51 with 850 $\mu$ m contour superimposed. The contour levels are 13.5 (=1.6 $\sigma$ ), 27, 40.5, 58.5, 72, 90 and 117 mJy/beam. 13.5 mJy/beam corresponds to 2.6 MJy sr^-1. This image clearly shows the extended 850 $\mu$ m disk. The small source to the north is the nucleus of NGC 5195.
Open with DEXTER

$\begin{figure} \par {\includegraphics[width=8.4cm,clip]{0469fig4.ps} } \end{figure}$	Figure 3: The model exponential disk (crosses) compared to the actual emission of the M 51 disk (solid line), for $h_{\rm d}=7.65$ kpc, $h_{\rm s}=3.15$ kpc, $L=1.1\times 10^{11}\ L_\odot$ , $\tau _{V,f}=4.35$ and no CO contamination.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0469fig5.ps} } \end{figure}$	Figure 4: Resulting optical depth for different luminosities assuming either zero CO contamination ( upper line) or an omnipresent maximum 12 per cent contamination ( lower line). The shaded area shows the possible solutions.
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$\begin{figure} \par {\includegraphics[width=8.8cm, clip]{0469fig6.ps} } \end{figure}$	Figure 5: Radial temperature profile for a total luminosity for M 51 of $L=1.1\times 10^{11}~L_\odot$ . The solid line marks zero CO contamination, the dotted line a maximum 12 per cent contamination, and the dashed line a contamination decreasing from maximum in the center to zero at the outer edge of M 51.
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$\begin{figure} \par {\includegraphics[width=8.8cm, clip]{0469fig7.ps} } \end{figure}$	Figure 6: The dust surface density profiles for a graphite and silicate ratio of 0.5:0.5 and $\kappa_{850} = 1.2~\rm g^{-1}~\rm cm^{2}$ ; no CO contribution (solid line), 12 percent CO contribution (dotted line) and decreasing CO contribution (dashed line).
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