Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0774fig1New.eps}\par\end{figure}$ Figure 1: Emission spectra of the 2-1 and 3-2 lines of SiO detected in the inner 3 kpc of NGC 1068. Four starred markers, overlaid on the CO(1-0) integrated intensity map of Schinnerer et al. (2000), highlight the central positions of the beams in the disk where we searched for SiO emission: the central offset (0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ) coincides with the position of the AGN, given by the S1 compact radio-source of Gallimore et al. (1996b) ( $\alpha _{2000}=02^{{\rm h}}$ 42 $^{{\rm m}}$ 40 $~\hbox{$.\!\!^{\rm s}$ }$ 71, $\delta _{2000}= -00$ $^$00 $^\prime$ 47.9 $^{\prime \prime }$ ), while offsets N, S and E probe the SiO emission over the starburst ring. Emission in the H¹³CO⁺(1-0) and HCO(1-0) lines is detected in the CND and over the starburst ring. The circles represent the beam sizes at 130.3 GHz (19 $^{\prime \prime }$ ) and 86.8 GHz (28 $^{\prime \prime }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0774fig2.eps}\end{figure}$ Figure 2: Top and middle: HCO⁺(1-0) and HOC⁺(1-0) spectra of the CND of NGC 1068. Bottom: HCO⁺(1-0)-to-HOC⁺(1-0) temperature ratio profile derived for channels fulfilling T[HOC⁺(1-0)] $>2\sigma$ . Error bars are $\pm \sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0774fig3.eps}\end{figure}$ Figure 3: Top panel: integrated intensity maps of CO(1-0) toward the CND of NGC 1068 obtained for the blue (thin contours: from 6 $\sigma$ by steps of 3 $\sigma$ ; $\sigma =0.67$ K km s^-1) and red (thick contours: same levels with $\sigma =0.47$ K km s^-1) emission components as defined in text (see also bottom panel). The maps have been derived from the data of Schinnerer et al. (2000). The starred marker highlights the AGN locus. Bottom panel: integrated spectrum of CO(1-0) emission in the CND. The W and E knots in the CO map correspond, respectively, to the red and blue components in the spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{0774fig4.eps}\end{figure}$ Figure 4: Molecular lines in the CND. Sub-panels are labeled with the name of the line displayed. Sub-panels 1 to 3 are derived from interferometer data (Tacconi et al. 1994, 1997; Schinnerer et al. 2000); panels 4 to 9 show single-dish spectra observed towards the nucleus (temperatures corrected by dilution effects assuming that the emission is coming from the CND). Two vertical point-dashed lines at $v-v_{{\rm sys}}=-185$ km s^-1 and 155 km s^-1, delimit the blue and red kinematical components. For each line, the blue-to-red (east-to-west) average brightness temperature ratio ( $R_{{\rm E/W}}$ ) is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0774fig5.eps} \end{figure}$ Figure 5: Temperature ratio profiles derived from spectra of Table 4. The left panel shows the CO(2-1)-to-CO(1-0) ratio, and the right panel the HCN(1-0)-to-CO(1-0) ratio. Error bars are $\pm 3\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{0774fig6.eps}\end{figure}$ Figure 6: LVG estimates for oxygenated species in the E/W knots of the CND. a1) For CO, continuous (pointed) curves are contours of constant 1-0 line temperature ((4-3)-to-(1-0) line ratio). a2) For SiO, same for 2-1 line temperature ((3-2)-to-(2-1) line ratio). a3) For H¹²CO⁺, same for 1-0 line temperature ([H¹²CO⁺]-to-H¹³CO⁺] 1-0 line ratio). a4) For HOC⁺, same for 1-0 line temperature. Squared (starred) markers show solutions for the East (West) knot.
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In the text

$\begin{figure} \par\includegraphics[width=7.48cm,clip]{0774fig7.eps} \par\end{figure}$ Figure 7: LVG estimates for non-oxygenated species in the E/W knots of the CND. b1) For HCN, continuous (pointed) lines are contours of constant 1-0 line temperature ((4-3)-to-(1-0) line ratio). b2) For CS, same for 2-1 line temperature. b3) For CN, same for 2-1/high freq. line temperature ((2-1/high freq.)-to-(2-1/low freq.) ratio); a range of possible solutions found is highlighted in bold face: we impose $n(\rm H_2)<10^6$ cm^-3 for consistency with the results from others species and allow for a $\pm$ 2 $\sigma$ uncertainty in the measured ratio. Markers are as is Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0774fig8.eps}\end{figure}$ Figure 8: Top panel: steady state HCO⁺-to-HOC⁺ abundance ratio as a function of the ionization degree of molecular gas. Curves for single formation paths are plotted; the thick line shows the predicted ratio for a XDR chemistry. Bottom panel: fraction of HCO⁺ and HOC⁺ molecules formed along each chemical path in a XDR chemistry.
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In the text

$\begin{figure} \par\resizebox{11.7cm}{!} { \includegraphics[angle=0,clip]{0774fig9.eps} }\end{figure}$ Figure 9: X-ray emission and molecular gas inthe CND: overlay of the distribution of hardX-ray emission in the 6-8 keV band (gray scale adapted from Ogle et al. 2003: whiter shades stand for stronger emission) and the CO(1-0) integrated emission as in Fig. 3. The AGN locus is highlighted by the starred marker.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0774fig2.eps}\end{figure}$	Figure 2: Top and middle: HCO⁺(1-0) and HOC⁺(1-0) spectra of the CND of NGC 1068. Bottom: HCO⁺(1-0)-to-HOC⁺(1-0) temperature ratio profile derived for channels fulfilling T[HOC⁺(1-0)] $>2\sigma$ . Error bars are $\pm \sigma$ .
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0774fig5.eps} \end{figure}$	Figure 5: Temperature ratio profiles derived from spectra of Table 4. The left panel shows the CO(2-1)-to-CO(1-0) ratio, and the right panel the HCN(1-0)-to-CO(1-0) ratio. Error bars are $\pm 3\sigma$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0774fig8.eps}\end{figure}$	Figure 8: Top panel: steady state HCO⁺-to-HOC⁺ abundance ratio as a function of the ionization degree of molecular gas. Curves for single formation paths are plotted; the thick line shows the predicted ratio for a XDR chemistry. Bottom panel: fraction of HCO⁺ and HOC⁺ molecules formed along each chemical path in a XDR chemistry.
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$\begin{figure} \par\resizebox{11.7cm}{!} { \includegraphics[angle=0,clip]{0774fig9.eps} }\end{figure}$	Figure 9: X-ray emission and molecular gas inthe CND: overlay of the distribution of hardX-ray emission in the 6-8 keV band (gray scale adapted from Ogle et al. 2003: whiter shades stand for stronger emission) and the CO(1-0) integrated emission as in Fig. 3. The AGN locus is highlighted by the starred marker.
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