Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi01.eps}}} \end{figure}$ Figure 1: Optical image (taken from the DSS survey) superimposed with the integrated CO(1-0) contours (white) obtained at the PdBI, with added short spacings from the IRAM 30 m telescope (see Sects. 4.2 and 4.3). Contour levels as in Fig. 14.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi02.eps}}} \end{figure}$ Figure 2: Positions of the IRAM 30 m observations are plotted with black crosses, and mosaic fields of the PdBI observations are shown as circles indicating the 42'' primary beam size for each observing field. The 30 m beamsize is shown in the upper left.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi03.eps} \end{figure}$ Figure 3: Continuum emission of the single field observations at 3 mm ( left) and 1 mm ( right). The white cross indicates the position at 18 cm with EVN. Contour levels are from 2 $\sigma$ (2 $\sigma$ ) = 1.0 (1.6) ${\rm mJy~beam^{-1}}$ to 9 (9.6) ${\rm mJy~beam^{-1}}$ in steps of 4 $\sigma$ (2 $\sigma$ ) at 3 mm (1 mm). Beam sizes are indicated at lower left.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi04.eps} \end{figure}$ Figure 4: PdBI central maps of the velocity integrated CO(1-0) ( left) and CO(2-1) ( right) emission in NGC 3718 (from velocities $\sim$ -300 to $\sim$ +300 km s^-1). Contour levels are from 3 $\sigma$ (3 $\sigma$ ) = 1.5 (2.7) to 5 (7.2) Jy beam^-1 km s^-1 in steps of $1\sigma$ (1 $\sigma$ ) for CO(1-0) (CO(2-1)). The white cross indicates the position at 18 cm with the European VLBI Network (EVN; Krips et al. 2005, in prep.).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1731fi05.eps} \end{figure}$ Figure 5: The Spectral Energy Distribution (SED) of NGC 3718. IR and optical fluxes with their errors are shown for completeness (taken from NED). The cm fluxes were observed with the VLA (FIRST: Becker et al. 1995; Nagar et al. 2001, 2002) and thus have an angular resolution comparable to the PdBI maps. The mm fluxes for both observing epochs are plotted (upper limit at 1 mm). The solid line indicates a fit ( $f_\nu \propto \nu ^\alpha$ ) with $\alpha =-0.01\pm 0.1$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1731fi06.eps} \includegraphics[angle=-90,width=8.8cm,clip]{1731fi07.eps} \end{figure}$ Figure 6: CO(1-0) ( upper panel) and CO(2-1) ( upper panel) spectra of the central emission in NGC 3718 observed with the PdBI (dark grey; integrated over the emission area), the IRAM 30 m telescope (light grey; Pott et al. 2004). The short-spacing corrected spectrum is also shown (dashed line; integrated over the emission area). Spectra are continuum subtracted. The rms noise level is here $\sim$ 4 mJy ( $\sim$ 6 mJy) for the PdBI data for CO(1-0) (CO(2-1)) ( $\Delta v=13$ km s^-1 for both).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi08.eps} \includegraphics[angle=-90,width=16cm,clip]{1731fi09.eps} \end{figure}$ Figure 7: Mean velocity fields of the CO(1-0) ( upper left) and CO(2-1) ( lower left) lines with their respective position-velocity maps (CO(1-0): upper right; CO(2-1) lower right) taken along the axis indicated in the maps ( solid line: major axis). The grey scale in the images on the right is the integrated line emission of CO(1-0) and CO(2-1) respectively. The light grey stars in the lower right panel illustrate the positions of the CO(1-0) components identified in the upper right panel. Left: velocity contours are in steps of 25 km s^-1 for CO(1-0) and for CO(2-1). Right: contour levels are in steps of 10% from the peak starting at 30%. The position velocity maps were Hanning smoothed.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.1cm,clip]{1731fi10.eps} \end{figure}$ Figure 8: PdBI central maps corrected with 30 m data for short-spacing effects of the integrated CO(1-0) ( left) and CO(2-1) ( right) emission in NGC 3718 at same size. Contour levels are from 5 $\sigma$ (3 $\sigma$ ) = 2.0 (2.4) to 8.0 (10.4) Jy beam^-1 km s^-1 in steps of $3\sigma$ (2 $\sigma$ ) for CO(1-0) (CO(2-1)). The white cross indicates the position of the AGN radio continuum source at 18 cm derived from EVN data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.1cm,clip]{1731fi11.eps} \end{figure}$ Figure 9: Comparison of pv-diagram along axis shown in Fig. 7 between PdBI-only data for the central pointing ( left) and PdBI+30 m data for the central mosaic ( right). The asymmetry is lowered in the central mosaic map but does not disappear totally. Thus, it cannot be totally due to missing short spacings. Contour levels are in steps of 10% from the peak starting at 30%. The position velocity maps were Hanning smoothed.
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In the text

$\begin{figure} \par\resizebox{88mm}{!}{\rotatebox{-90}{\includegraphics{1731fi12... ...esizebox{6.5cm}{!}{\rotatebox{-90}{\includegraphics{1731fi13.eps}}} \end{figure}$ Figure 10: PdBI mosaic map of the velocity integrated CO(1-0) emission in NGC 3718 (upper figure; from -300 to +300 km s^-1). Spectra are shown in the lower panel. Contour levels are from $2\sigma =1.0$ Jy beam^-1 km s^-1 to 4 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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In the text

$\begin{figure} \par\resizebox{88mm}{!}{\rotatebox{-90}{\includegraphics{1731fi14... ...esizebox{6.5cm}{!}{\rotatebox{-90}{\includegraphics{1731fi15.eps}}} \end{figure}$ Figure 11: Velocity integrated intensity map of the CO(1-0) emission for the combined PdBI+30 m data (fromm -300 to +300 km s^-1). Contour levels are from $2\sigma =1.0$ Jy beam^-1 km s^-1 to 6.0 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi16.eps}}} \end{figure}$ Figure 12: Tilt angles $\omega (r)$ . The old model of Pott et al. (2004) is given as a solid line, while a dashed line is used for our new model.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi17.eps}}} \end{figure}$ Figure 13: The integrated intensity map of our model is plotted here, before spatial filtering to match the response of the interferometer and single dish telescope.
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In the text

$\begin{figure} \par\resizebox{8.65cm}{!}{\rotatebox{-90}{\includegraphics{1731fi... ...sizebox{8.65cm}{!}{\rotatebox{-90}{\includegraphics{1731fi20.eps}}} \end{figure}$ Figure 14: Model vs. observation. Integrated maps of the PdBI data only ( upper panel), the PdBI and 30 m data combined ( middle panel) and the 30 m data only ( lower panel). The model (grey scale) is overlaid with solid contours of the observed data. Contour levels: PdBI-only $2\sigma =1.0$ to 4 Jy beam^-1 km s^-1 by $1\sigma$ ; PdBI+30 m $2\sigma =1.0$ to 6.0 Jy beam^-1 km s^-1 by $1\sigma$ ; 30 m-only $3\sigma =1.0$ to 10 by 1.0 Jy beam^-1 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi21.eps} \in... ...fi22.eps} \includegraphics[angle=-90,width=16cm,clip]{1731fi23.eps} \end{figure}$ Figure 15: Model vs. Observation. Integrated maps of the measured ( left) and simulated ( right) PdBI+30 m data restricted to the following velocity ranges: -250 to -80 km s^-1 ( upper panel), -80 to 80 km s^-1 ( middle panel), and 80 to 225 km s^-1 ( lower panel). Contour levels are $3\sigma =1.2$ ${\rm Jy~beam^{-1}~km~s^{-1}}$ in steps of $1\sigma$ .
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{-90}{\includegraphics{1731fi24... ...{!}{\rotatebox{-90}{\includegraphics{1731fi25.eps}}}\hspace*{4mm}} \end{figure}$ Figure 16: Upper panels: the short-spacing corrected images of the observed data ( left) and of the model ( right) data. Lower panels: 30 m spectra at positions of the CO peaks. Contour levels are from $2\sigma =1.0$ to 6.0 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi2... ...esizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi27.eps}}} \end{figure}$ Figure 17: Upper panels: observed data, with first order moment maps ( left) and position velocity cuts ( right) taken along the axis indicated in the first order moment map (going through the AGN). Lower panels: same as above for the model. The area within the dashed box is identical with the map shown in the right panel of Fig. 9. Contour levels are in steps of 10% from the peak starting at 20%. The position velocity maps were Hanning smoothed.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi01.eps}}} \end{figure}$	Figure 1: Optical image (taken from the DSS survey) superimposed with the integrated CO(1-0) contours (white) obtained at the PdBI, with added short spacings from the IRAM 30 m telescope (see Sects. 4.2 and 4.3). Contour levels as in Fig. 14.
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$\begin{figure} \resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi02.eps}}} \end{figure}$	Figure 2: Positions of the IRAM 30 m observations are plotted with black crosses, and mosaic fields of the PdBI observations are shown as circles indicating the 42'' primary beam size for each observing field. The 30 m beamsize is shown in the upper left.
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$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi03.eps} \end{figure}$	Figure 3: Continuum emission of the single field observations at 3 mm ( left) and 1 mm ( right). The white cross indicates the position at 18 cm with EVN. Contour levels are from 2 $\sigma$ (2 $\sigma$ ) = 1.0 (1.6) ${\rm mJy~beam^{-1}}$ to 9 (9.6) ${\rm mJy~beam^{-1}}$ in steps of 4 $\sigma$ (2 $\sigma$ ) at 3 mm (1 mm). Beam sizes are indicated at lower left.
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$\begin{figure} \par\resizebox{88mm}{!}{\rotatebox{-90}{\includegraphics{1731fi12... ...esizebox{6.5cm}{!}{\rotatebox{-90}{\includegraphics{1731fi13.eps}}} \end{figure}$	Figure 10: PdBI mosaic map of the velocity integrated CO(1-0) emission in NGC 3718 (upper figure; from -300 to +300 km s^-1). Spectra are shown in the lower panel. Contour levels are from $2\sigma =1.0$ Jy beam^-1 km s^-1 to 4 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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$\begin{figure} \par\resizebox{88mm}{!}{\rotatebox{-90}{\includegraphics{1731fi14... ...esizebox{6.5cm}{!}{\rotatebox{-90}{\includegraphics{1731fi15.eps}}} \end{figure}$	Figure 11: Velocity integrated intensity map of the CO(1-0) emission for the combined PdBI+30 m data (fromm -300 to +300 km s^-1). Contour levels are from $2\sigma =1.0$ Jy beam^-1 km s^-1 to 6.0 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi16.eps}}} \end{figure}$	Figure 12: Tilt angles $\omega (r)$ . The old model of Pott et al. (2004) is given as a solid line, while a dashed line is used for our new model.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{1731fi17.eps}}} \end{figure}$	Figure 13: The integrated intensity map of our model is plotted here, before spatial filtering to match the response of the interferometer and single dish telescope.
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$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1731fi21.eps} \in... ...fi22.eps} \includegraphics[angle=-90,width=16cm,clip]{1731fi23.eps} \end{figure}$	Figure 15: Model vs. Observation. Integrated maps of the measured ( left) and simulated ( right) PdBI+30 m data restricted to the following velocity ranges: -250 to -80 km s^-1 ( upper panel), -80 to 80 km s^-1 ( middle panel), and 80 to 225 km s^-1 ( lower panel). Contour levels are $3\sigma =1.2$ ${\rm Jy~beam^{-1}~km~s^{-1}}$ in steps of $1\sigma$ .
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$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{-90}{\includegraphics{1731fi24... ...{!}{\rotatebox{-90}{\includegraphics{1731fi25.eps}}}\hspace*{4mm}} \end{figure}$	Figure 16: Upper panels: the short-spacing corrected images of the observed data ( left) and of the model ( right) data. Lower panels: 30 m spectra at positions of the CO peaks. Contour levels are from $2\sigma =1.0$ to 6.0 Jy beam^-1 km s^-1 in steps of $1\sigma$ .
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