All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{0482fig1.eps} \end{figure}$ Figure 1: Channel maps of the C I $(^3{\rm P}_2 \to ~\!^3{\rm P}_1)$ line of F10214 after subtracting the continuum. The contours are -3, -2, 2, 3, 4, 5, 6, 7 $\times$ 2.7 mJy beam^-1 (1 $\sigma$ ), with a synthesized beam of 1.12 $\hbox {$^{\prime \prime }$ }$ $\times$ 0.97 $\hbox {$^{\prime \prime }$ }$ , which is shown in the lower left corner of the first panel. The maps are centered on the position shown as a cross ( $\alpha$ (J2000) = 10 $\rm ^h$ 24 $\rm ^m$ 34 $.\!\!^{\rm s}$ 56, $\delta$ (J2000) = +47 $\rm ^o$ 09 $\hbox {$^\prime $ }$ 09 $.\!\!^{\prime\prime}$ 8), here and in subsequent figures.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{0482fig2.eps} \end{figure}$ Figure 2: Left panel: contour map of the 1.2 mm continuum towards F10214, which was created from the line free channels. Contours are -3, 3, 5, 7, 9, 11 $\times$ 0.7 mJy beam^-1 (1 $\sigma$ ). Right panel: contour map of the C I $(^3{\rm P}_2 \to ~\!^3{\rm P}_1)$ line integrated intensity towards F10214 after subtracting the continuum overlaid by the velocity field in color map. Contours are -3, 3, 6, 9, 12, 15, 20 $\times$ 0.081 Jy km s^-1 beam^-1 (1 $\sigma$ ). A synthesized beam of 1.12 $\hbox {$^{\prime \prime }$ }$ $\times$ 0.97 $\hbox {$^{\prime \prime }$ }$ is shown in the lower left corner of the figures.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{0482fig3.eps} \end{figure}$ Figure 3: CO(3-2) channel maps of F10214 after subtracting the continuum. The contours are -3, -2, 2, 3, 4, 5, 6, 7, 8, 9 $\times$ 1.9 mJy beam^-1 (1 $\sigma$ ), with a synthesized beam of 4.9 $\hbox {$^{\prime \prime }$ }$ $\times$ 3.3 $\hbox {$^{\prime \prime }$ }$ , which is shown in the lower left corner of the first panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{0482fig4.eps} \end{figure}$ Figure 4: Left panel: contour map of the 3 mm continuum towards F10214, which was created from the line free channels. Contours are -2, 2, 3 $\times$ 0.17 mJy beam^-1 (1 $\sigma$ ). Right panel: contour map of the CO(3-2) line integrated intensity towards F10214 after subtracting the continuum overlaid by the velocity field in color map. Contours are -3, 3, 9, 15, 30, 50 $\times$ 0.038 Jy km s^-1 beam^-1 (1 $\sigma$ ). The synthesized beams of 6.5 $\hbox {$^{\prime \prime }$ }$ $\times$ 3.8 $\hbox {$^{\prime \prime }$ }$ and 4.9 $\hbox {$^{\prime \prime }$ }$ $\times$ 3.3 $\hbox {$^{\prime \prime }$ }$ are shown in the lower left corner of the figures.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{0482fig5.eps} \end{figure}$ Figure 5: Spectra of the averaged profile and the CO 3-2, 4-3, 6-5, 7-6, C I $(^3{\rm P}_1 \to ~\! ^3{\rm P}_0)$ and C I $(^3{\rm P}_2 \to ~\!^3{\rm P}_1)$ lines towards F10214. The results from the PdBI are shown in the two panels at the lower right. All lines are fitted and Gaussian fits are shown as continuous lines for which the FWHM line width and the central velocity are fixed to the value determined from the averaged CO profile. The dashed horizontal lines in the PdBI spectra show the dust continuum levels. The zero and Gaussian fitted velocities from the averaged CO profile are shown as dashed vertical lines. The C I $(^3{\rm P}_1 \to ~\! ^3{\rm P}_0)$ spectrum is taken from Weiß et al. (2005a).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0482fig6.eps} \end{figure}$ Figure 6: Observed CO fluxes vs. rotational quantum number (CO line SED, filled squares) for F10214 fitted by the a single component LVG model with n(H₂) = 10^3.8 cm^-3 and $T_{\rm kin}$ = 60 K, shown as a thick solid line. Other measurements, taken from the literatures, are marked by different symbols. For better visibility, previous data points for the 3-2 line are shown with small x-axis offsets.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0482fig7.eps} \end{figure}$ Figure 7: Reduced $\chi ^2$ distribution for a single component LVG model fit to the observed line luminosity ratios (grey scale and white contours, contours: $\chi ^2$ = 0.5, 1, 2, 4). The CO abundance per velocity gradient for the LVG models is [CO]/ ${({\rm d}v/{\rm d}r)}$ = 1 $\times$ $10^{-5}~{\rm pc}~(\rm km~s^{-1})^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0482fig8.eps} \end{figure}$ Figure 8: Two component dust model for F10214. Displayed flux densities were taken from Lawrence et al. 1993 (20 cm, 6 cm and 3.6 cm, open squares), this work (3 mm and 1.2 mm, open circles), Downes et al. 1992 (1200, 100 $\mu$ m, filled triangles), Rowan-Robinson et al. 1993 (1100, 800, 450 $\mu$ m, filled circles), Benford et al. 1999 (350 $\mu$ m, open triangle) and Rowan-Robinson et al. 1991 (60 $\mu$ m, filled square). The dashed lines show the thermal dust continuum emission for 80 and 160 K dust components. The solid line is the total emission from both components. See Sect. 4.6 for the details of the dust models.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0482fig9.eps} \end{figure}$ Figure 9: Comparison of the CO line SEDs of selected local and high-zgalaxies. The SEDs are shown for IRAS F10214+4724 (thick solid line, as shown in Fig. 6), APM 08279+5255 (z = 3.9, Weiß et al. 2007), BR 1202-0725 (z = 4.7, Riechers et al. 2006), SDSS J1148+5251 (z = 6.4, Bertoldi et al. 2003; Walter et al. 2003), the high-excitation component in the center of M 82 (Weiß et al. 2005c), NGC 253 center (Güsten et al. 2006), SMM J16359+6612 (z = 2.5, Weiß et al. 2005b) and the Galactic Center (solid circles, Fixsen et al. 1999). The CO line SEDs are normalized by their CO(1-0) flux density.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{0482fig3.eps} \end{figure}$	Figure 3: CO(3-2) channel maps of F10214 after subtracting the continuum. The contours are -3, -2, 2, 3, 4, 5, 6, 7, 8, 9 $\times$ 1.9 mJy beam^-1 (1 $\sigma$ ), with a synthesized beam of 4.9 $\hbox {$^{\prime \prime }$ }$ $\times$ 3.3 $\hbox {$^{\prime \prime }$ }$ , which is shown in the lower left corner of the first panel.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0482fig7.eps} \end{figure}$	Figure 7: Reduced $\chi ^2$ distribution for a single component LVG model fit to the observed line luminosity ratios (grey scale and white contours, contours: $\chi ^2$ = 0.5, 1, 2, 4). The CO abundance per velocity gradient for the LVG models is [CO]/ ${({\rm d}v/{\rm d}r)}$ = 1 $\times$ $10^{-5}~{\rm pc}~(\rm km~s^{-1})^{-1}$ .
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