All Figures

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=6cm,clip]{8341_1.eps}\... ...8341_2.eps}\includegraphics[angle=-90,width=6cm,clip]{8341_3.eps} } \end{figure}$ Figure 1: Velocity integrated intensities of [C I] emission (color) overlayed with contours of a) ¹²CO 4-3, b) ¹²CO 1-0 and c) ¹³CO 1-0 integrated intensities at a common angular resolution of 70 $^{\prime \prime }$ . The center of the maps is at $\alpha =03^{\rm h}44^{\rm m}10^{\rm s}$ , $\delta = 32 \hbox {$^\circ $ }06 \hbox {$^\prime $ }$ (J2000). All tracers are integrated from $V_{\rm LSR}$ 2 km s^-1 to 14 km s^-1. Contours range between 20% to 90% with a step of 10% of the peak intensities that are 73 K km s^-1 for ¹²CO 4-3, 72 K km s^-1 for ¹²CO 1-0 and 31 K km s^-1 for ¹³CO 1-0. The seven filled triangles indicates the positions where we carry out a detailed PDR analysis later. The open pentacle symbol denotes the position of HD 281159.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17cm,clip]{8341_4.eps}\end{figure}$ Figure 2: Spectra of the four different tracers on those six positions along the cut from the northern edge of the cloud into the cloud, and on the seventh position at the south of the cloud. [C I] spectra in all the positions have been multiplied by 3. All panels have the same x axis from 3.5 km s^-1 to 14.5 km s^-1 and the same y axis from -0.5 K to 30.5 K.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_5.eps} \end{figure}$ Figure 3: The top panel a) presents the normalized integrated intensities of [C I], ¹²CO 4-3, ¹²CO 1-0 and ¹³CO 1-0 in the seven selected positions. The typical errors of the intensities are about 15%, resulting in errors of the line ratios of about 21%; b) displays integrated line intensity ratios. The x axes of all panels are the relative distance to the northern rim (8 $^\prime$ , 6 $^\prime$ ) position. The southern rim is plotted in a separate box.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_6.eps}\end{figure}$ Figure 4: The color plot represents the ¹²CO 4-3 / ¹²CO 1-0 line intensity ratio (in units of K km s^-1) observed in the IC 348 cloud. The contours show the ¹²CO 4-3 line intensity spaced at 10% intervals from 20% to 90% relative to the peak intensity of 73 K km s^-1. White pixels in the figure denote positions where either of the line intensities falls below the 3 $\sigma$ threshold.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_7.eps}\end{figure}$ Figure 5: The C/CO column density ratio overlaid by ¹³CO 1-0 integrated intensities contours. The contour levels are spaced at 10% intervals from 20% to 90% relative to the peak intensity of 31 K km s^-1. White pixels in the figure denote positions where the ¹³CO 1-0 intensities fall below the 3 $\sigma$ threshold.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_8.eps} \end{figure}$ Figure 6: FUV intensity distribution (contours) in IC 348 estimated from the IRAS FIR fluxes, overlayed on the [C I] integrated intensities (colors). The FUV intensity $\chi _{\rm FIR}$ contour levels run from 5, 10, 20 to 100 by steps of 20 Draine units, $\chi _{0}$ .
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{8431_9.eps}\includegraphics[angle=-90,width=7cm,clip]{8431_10.eps} } \end{figure}$ Figure 7: Comparison of the observed line intensity ratios [C I]/¹²CO 4-3, [C I]/¹³CO 1-0 and ¹²CO 4-3/¹²CO 1-0 at (1 $^\prime$ , -1 $^\prime$ ) with the single clump KOSMA - $\tau$ PDR model calculations. The left figure shows the fit of clump mass and density at a fixed FUV field $\chi$ of 10^1.5; the right one presents the fit of FUV field and clump density at a fixed clump mass of 10 $^{-1}~M_{\odot}$ . The central solid contours represent the observed intensity ratios, the outer dashed two give those for a 20% uncertainty. The grey-scale images indicate the reduced $\chi ^{2}$ of the fit. The position of the minimum reduced $\chi ^{2}$ is marked by a white cross. The horizontal light blue line in the right panel shows the FUV flux $\chi _{\rm FIR}$ from the HIRES data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=0,clip]{8431_11.eps}\includegraphics[width=8cm,angle=0]{8431_12.eps}\end{figure}$ Figure 8: Observed (filled symbols) and modelled line intensities of ¹²CO, ¹³CO, and [C I] from both Ensemble case 1 (drawn lines with open symbols) and Ensemble case 2 (dotted lines, open symbols with a cross inside) at the northern rim ( left panel) and the southern rim ( right panel). To better display the data, we artificially shift the [C I] frequency by +40 GHz for the observed intensity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17cm,clip]{8341_4.eps}\end{figure}$	Figure 2: Spectra of the four different tracers on those six positions along the cut from the northern edge of the cloud into the cloud, and on the seventh position at the south of the cloud. [C I] spectra in all the positions have been multiplied by 3. All panels have the same x axis from 3.5 km s^-1 to 14.5 km s^-1 and the same y axis from -0.5 K to 30.5 K.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_6.eps}\end{figure}$	Figure 4: The color plot represents the ¹²CO 4-3 / ¹²CO 1-0 line intensity ratio (in units of K km s^-1) observed in the IC 348 cloud. The contours show the ¹²CO 4-3 line intensity spaced at 10% intervals from 20% to 90% relative to the peak intensity of 73 K km s^-1. White pixels in the figure denote positions where either of the line intensities falls below the 3 $\sigma$ threshold.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_7.eps}\end{figure}$	Figure 5: The C/CO column density ratio overlaid by ¹³CO 1-0 integrated intensities contours. The contour levels are spaced at 10% intervals from 20% to 90% relative to the peak intensity of 31 K km s^-1. White pixels in the figure denote positions where the ¹³CO 1-0 intensities fall below the 3 $\sigma$ threshold.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8431_8.eps} \end{figure}$	Figure 6: FUV intensity distribution (contours) in IC 348 estimated from the IRAS FIR fluxes, overlayed on the [C I] integrated intensities (colors). The FUV intensity $\chi _{\rm FIR}$ contour levels run from 5, 10, 20 to 100 by steps of 20 Draine units, $\chi _{0}$ .
Open with DEXTER