Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3301fig1.ps} \end{figure}$ Figure 1: Interferometric maps of the Class 0 protostar NGC 7129-FIRS 2 in the continuum at 1 mm and 3 mm, and the following molecular lines: CH₃CN 5 $\rightarrow$ 4, D₂CO 4₀₄ $\rightarrow$ 3₀₃, CH₃OH 5_1,4 $\rightarrow$ 4_1,4. The panel marked with "CH₃OH (high)'' shows the integrated intensity map of the lines 5_3,1 $\rightarrow$ 4_3,1, 5_3,2 $\rightarrow$ 4_3,2,5_2,2 $\rightarrow$ 4_2,2, and 5_3,3 $\rightarrow$ 4_3,3. Contour levels are: a) 10 to 60 by 5 mJy/beam; b) 20 to 160 by 20 mJy/beam; c) 0.6 to 2.7 by 0.3 Jy/beam km s^-1; d) 0.3 to 0.6 by 0.1 Jy/beam km s^-1; e) 1 to 4 by 0.5 Jy/beam km s^-1; f) 1 to 7.5 by 0.5 Jy/beam km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{3301fig2.eps} \end{figure}$ Figure 2: Continuum visibilities at 92 GHz and 230 GHz vs. projected baselines in units of wavelength. In the bottom panel we show the 92 GHz and the 230 GHz visibilities together. The 92 GHz visibilities were scaled by a factor of 10.5 to match the 230 GHz ones. The perfect match between the 92 GHz and 230 GHz visibilities suggests that both emissions arise in the same region as expected in the case of dust thermal emission.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{3301fig3.ps} \end{figure}$ Figure 3: Comparison between the single-dish (thin histograms) and interferometric (thick histograms) spectra towards the hot core position. The interferometric spectrum was scaled for an easier comparison. Note that we recovered all the flux for the CH₃CN line with the highest upper state energy.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3301fig4.ps} \end{figure}$ Figure 4: Rotational diagram of CH₃OH towards the hot core and the outflow condensation. Note that the rotation temperature towards the hot core is much higher than towards the outflow condensation.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{3301fig5.ps} \end{figure}$ Figure 5: Spectra of the upper side band (USB) and lower side band (LSB) of the 1 mm receiver obtained in our PdBI observations with our best guess for line identifications. For clarity, we divided the molecular species in three groups. The first group is formed by the more reliable identifications and S¹⁸O. Beginning from the top, in the first line of panels we compare the observed spectra with the synthesized ones taking only this first group into account. In the second line, we add CH₃OCHO-A/E and show the obtained synthesized spectra. Inclusion of these compounds improves agreement with the observational data. However, the large CH₃OCHO-A/E abundance we derived from these observations raise some questions about this identification. In the third line of panels, we show the synthesized spectra after adding some other exotic compounds. The last line shows the residual spectra after subtracting our fit. Note that agreement between the synthesized and observed one is very good in the USB, but some lines remain unidentified in the LSB.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3301fig6.ps} \end{figure}$ Figure 6: Single-dish spectra of the H₂CO 3₁₂ $\rightarrow$ 2₁₁ and D₂CO 4₀₄ $\rightarrow$ 3₀₃ lines towards FIRS 2. In the bottom panel we show the I(D₂CO 4₀₄ $\rightarrow$ 3₀₃)/I(H₂CO 3₁₂ $\rightarrow$ 2₁₁) line ratio. Note that this ratio presents a minimum around the velocity of the ambient cloud ( $\sim$ -10 km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3301fig7.ps} \end{figure}$ Figure 7: Relative abundances of the complex O- and N-bearing molecules as a function of the protostellar luminosity for the objects listed in Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{3301fig3.ps} \end{figure}$	Figure 3: Comparison between the single-dish (thin histograms) and interferometric (thick histograms) spectra towards the hot core position. The interferometric spectrum was scaled for an easier comparison. Note that we recovered all the flux for the CH₃CN line with the highest upper state energy.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3301fig4.ps} \end{figure}$	Figure 4: Rotational diagram of CH₃OH towards the hot core and the outflow condensation. Note that the rotation temperature towards the hot core is much higher than towards the outflow condensation.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3301fig6.ps} \end{figure}$	Figure 6: Single-dish spectra of the H₂CO 3₁₂ $\rightarrow$ 2₁₁ and D₂CO 4₀₄ $\rightarrow$ 3₀₃ lines towards FIRS 2. In the bottom panel we show the I(D₂CO 4₀₄ $\rightarrow$ 3₀₃)/I(H₂CO 3₁₂ $\rightarrow$ 2₁₁) line ratio. Note that this ratio presents a minimum around the velocity of the ambient cloud ( $\sim$ -10 km s^-1).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3301fig7.ps} \end{figure}$	Figure 7: Relative abundances of the complex O- and N-bearing molecules as a function of the protostellar luminosity for the objects listed in Table 3.
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