All Figures

$\begin{figure} \par\includegraphics[width=16cm,angle=-90]{9545fig1.eps} \end{figure}$ Figure 1: ¹²CO(1-0) velocity channel maps observed with the IRAM PdBI+30 m in the nucleus of NGC 3147, with a spatial resolution of 1 $.\!\!^{\prime\prime}$ 9 $\times$ 1 $.\!\!^{\prime\prime}$ 6 (HPBW). The center of the maps, given in Table 1, is $\alpha _{2000}$ = 10 $^{\rm h}$ 16 $^{\rm m}$ 53.6 $^{\rm s}$ , $\delta _{2000}$ = 73 $^{\circ }$ 24 $^{\prime }$ 03 $^{\prime \prime }$ . Velocity channels range from $\Delta V = -230~{\rm km~s^{-1}}$ to $+220~{\rm km~s^{-1}}$ in steps of $10~{\rm km~s^{-1}}$ relative to $V_{\rm hel} = 2813~{\rm km~s^{-1}}$ . The contours begin at $5~{\rm mJy~beam^{-1}}$ , their spacing is $5~{\rm mJy~beam^{-1}}$ , and their maximum is $50~{{\rm mJy~beam}^{-1}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=16.3cm,angle=-90]{9545fig2.eps} \end{figure}$ Figure 2: Same as Fig. 1 but for the ¹²CO(2-1) line, with a spatial resolution of 1 $.\!\!^{\prime\prime}$ 6 $\times$ 1 $.\!\!^{\prime\prime}$ 4. The velocity range is the same as for Fig. 1. The contours begin at $10~{\rm mJy~beam^{-1}}$ , their spacing is $5~{\rm mJy~beam^{-1}}$ , and their maximum is $45~{\rm mJy~beam^{-1}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0,bb=47 145 590 680]{9545fig3.ps} \end{figure}$ Figure 3: Radial brightness profiles are shown in the top panel, with J given as a dotted line (blue), and IRAC $3.6~{\rm \mu}$ m as a solid one (red). Thevertical dashed line corresponds to 200 pc. The lower panels display the radial runs of ellipticity, $\epsilon$ , position angle $\theta$ , and cos( $4\theta$ ) terms inthe ellipse fitting residuals.
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In the text

$\begin{figure} \par\includegraphics[height=12.5cm,angle=-90]{9545fg4t.ps}\par\includegraphics[height=12.5cm,angle=-90]{9545fg4b.ps} \end{figure}$ Figure 4: Spectra maps of NGC 3147 made with the IRAM 30 m with $7^{\prime \prime }$ spacing in ¹²CO(1-0) ( top) and ¹²CO(2-1) ( bottom). The positions are offsets relative to the center of NGC 3147, whose coordinates are listed in Table 1. Each spectrum has a velocity scale from -500 to $500~{\rm km~s^{-1}}$ , and an antenna temperature scale ( $T^{*}_{\rm A}$ ) from -0.05 to $0.25~{\rm K}$ for ¹²CO(1-0) and to 0.20 K for ¹²CO(2-1).
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,angle=-90]{9545fig5.ps} \end{figure}$ Figure 5: HCN(1-0) spectrum towards the center of NGC 3147, averaged over the 9-point map made with the IRAM 30 m with $7^{\prime \prime }$ spacing.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90,bb=145 17 460 750]{9545fig6.eps} \end{figure}$ Figure 6: Left panel: ¹²CO(1-0) integrated intensity contours observed with the IRAM PdBI+30 m toward the center of NGC 3147. The cross marks the coordinates of the center as given in Table 1, with offsets in arcseconds. The rms noise level is $\sigma = 0.15~{\rm Jy~beam^{-1}~km~s^{-1}}$ . The map, derived with 2 $\sigma$ clipping, has not been corrected for primary beam attenuation. Contour levels run from 4 $\sigma$ to 17 $\sigma$ with 2.5 $\sigma$ spacing. In this map the full $\pm 240~{\rm km~s^{-1}}$ velocity range is used. The beam of 1 $.\!\!^{\prime\prime}$ 9 $\times$ 1 $.\!\!^{\prime\prime}$ 6 is plotted at lower left. Right panel: same for ¹²CO(2-1). The rms noise level is $\sigma = 0.2~{\rm Jy~beam^{-1}~km~s^{-1}}$ . Contour levels run from 5 $\sigma$ to 18 $\sigma$ with 2.5 $\sigma$ spacing. The beam of 1 $.\!\!^{\prime\prime}$ 4 $\times$ 1 $.\!\!^{\prime\prime}$ 2 is plotted at lower left.
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In the text

$\begin{figure} \par\hbox{ \includegraphics[width=8cm,angle=-90]{9545fg7l.ps}\includegraphics[width=8cm,angle=-90]{9545fg7r.ps} } \end{figure}$ Figure 7: Left panel: radial distribution (azimuthal average, deprojected to face-on orientation) of the ¹²CO(1-0) integrated intensity shown in Fig. 6. Right panel: same for ¹²CO(2-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90]{9545fig8.eps}\end{figure}$ Figure 8: ¹²CO(1-0) contours as in Fig. 6 ( left panel) superposed on the greyscale ¹²CO(2-1) map that has been tapered, convolved to the same resolution, and corrected for primary beam attenuation, in units of ${\rm Jy~beam^{-1}~km~s}^{-1}$ . The beam is plotted at lower left.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90]{9545fig9.eps}\end{figure}$ Figure 9: Contours and greyscale of the CO(2-1)/CO(1-0) ratio map. Contours run from 0.1 to 1.8 in steps of 0.1 in temperature units.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90]{9545fg10.eps} \end{figure}$ Figure 10: Overlay of the integrated ¹²CO(1-0) emission in grey scale, same as Fig. 6 ( left panel), with the CO mean-velocity field in contours spanning the range -200 km s^-1 to 200 km s^-1 in steps of 10 km s^-1. The velocities are referred to $V_{\rm hel} = 2813$ km s^-1. Solid (dashed) lines are used for positive (negative) velocities. The dotted line indicates the major axis (PA = 150 $^{\circ }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9545fg11.ps} \end{figure}$ Figure 11: ¹²CO(1-0) position-velocity (p-v) diagram along the major axis of NGC 3147 using the whole velocity range +/-240 km s^-1. The coordinates of the center (0, 0), the heliocentric velocity, and PA used are given in Table 1. Contour levels are from 3.2 to $32~{\rm mJy~beam^{-1}}$ in steps of $3.2~{\rm mJy~beam^{-1}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9545fg12.ps} \end{figure}$ Figure 12: ¹²CO(1-0) position-velocity (p-v) diagram along the minor axis of NGC 3147 using the same velocity range, center, PA, and systemic velocity as for Fig. 11. Contour levels are from 2.8 to $28~{\rm mJy~beam^{-1}}$ in steps of $2.8~{\rm mJy~beam^{-1}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f13c.eps} \end{figure}$ Figure 13: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the near-infrared J image from the CFHT, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f14c.eps} \end{figure}$ Figure 14: The J-K image from the CFHT with ¹²CO(2-1) integrated intensity overlaid in contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). North is up and east to the left.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f15c.eps} \end{figure}$ Figure 15: GALEX FUV sky subtracted image of NGC 3147. The central 120 $^{\prime \prime }$ of the galaxy are shown. The box shows the central 50 $^{\prime \prime }$ , field of view of our ¹²CO observations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f16c.eps} \end{figure}$ Figure 16: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the GALEX FUV image of NGC 3147, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f17c.eps}\end{figure}$ Figure 17: Spitzer/IRAC ``dust-only'' image at 8 $\mu$ m of NGC 3147. The central 120 $^{\prime \prime }$ of the galaxy are shown. The box shows the central 50 $^{\prime \prime }$ , field of view of our ¹²CO observations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f18b.eps}\end{figure}$ Figure 18: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the 8 $\mu$ m ``dust-only'' (Spitzer/IRAC) image of NGC 3147, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{9545f19.ps} \end{figure}$ Figure 19: Strengths (Q₁, Q₂, and total $Q_{\rm T}$ ) and phases ( $\phi _1$ and $\phi _2$ ) of the m=1 and m=2 Fourier components of the stellar potential inside a field of 48 $^{\prime \prime }$ in diameter (r < 4.6 kpc).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,bb=80 80 530 610]{9545f20.ps}\end{figure}$ Figure 20: CO(1-0) contours overlaid on the gravitational torque map (t(x, y) $\times$ $\Sigma$ (x, y), as defined in text) in the center of NGC 3147. The torque map (grey/color scale) is normalized to the maximum absolute value of the torques. The derived torques change sign as expected in a butterfly diagram, delineating four quadrants. The orientation of quadrants follows the bar orientation in NGC 3147. In this deprojected picture, the major axis of the galaxy is oriented parallel to the abscissa. The line reproduces the mean orientation of the bar (PA = 20 $^{\circ }$ on the deprojected image and 85 $^{\circ }$ on the projected one).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,bb=80 80 530 610]{9545f21.ps} \end{figure}$ Figure 21: Same as Fig. 20 for the ¹²CO(2-1) emission taken as a tracer of gas surface density.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm]{9545f22.ps} \end{figure}$ Figure 22: The torque, or more precisely the fraction of the angular momentum transferred from/to the gas in one rotation - dL/L - is plotted for ¹²CO(1-0) ( left) and ¹²CO(2-1) ( right).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{9545f23.ps} \end{figure}$ Figure 23: Model rotation curve and derived frequencies $\Omega$ , $\Omega -\kappa /2$ , and $\Omega +\kappa /2$ , for NGC 3147. The star symbols are the data derived from the CO kinematics, deprojected with an inclination of $i = 29.5^\circ$ . The horizontal line corresponds to $\Omega_{\rm p}~=~125$ km s^-1 kpc^-1.
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In the text

$\begin{figure} \par\includegraphics[width=16.3cm,angle=-90]{9545fig2.eps} \end{figure}$	Figure 2: Same as Fig. 1 but for the ¹²CO(2-1) line, with a spatial resolution of 1 $.\!\!^{\prime\prime}$ 6 $\times$ 1 $.\!\!^{\prime\prime}$ 4. The velocity range is the same as for Fig. 1. The contours begin at $10~{\rm mJy~beam^{-1}}$ , their spacing is $5~{\rm mJy~beam^{-1}}$ , and their maximum is $45~{\rm mJy~beam^{-1}}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=0,bb=47 145 590 680]{9545fig3.ps} \end{figure}$	Figure 3: Radial brightness profiles are shown in the top panel, with J given as a dotted line (blue), and IRAC $3.6~{\rm \mu}$ m as a solid one (red). Thevertical dashed line corresponds to 200 pc. The lower panels display the radial runs of ellipticity, $\epsilon$ , position angle $\theta$ , and cos( $4\theta$ ) terms inthe ellipse fitting residuals.
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$\begin{figure} \par\includegraphics[height=8.8cm,angle=-90]{9545fig5.ps} \end{figure}$	Figure 5: HCN(1-0) spectrum towards the center of NGC 3147, averaged over the 9-point map made with the IRAM 30 m with $7^{\prime \prime }$ spacing.
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$\begin{figure} \par\hbox{ \includegraphics[width=8cm,angle=-90]{9545fg7l.ps}\includegraphics[width=8cm,angle=-90]{9545fg7r.ps} } \end{figure}$	Figure 7: Left panel: radial distribution (azimuthal average, deprojected to face-on orientation) of the ¹²CO(1-0) integrated intensity shown in Fig. 6. Right panel: same for ¹²CO(2-1).
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$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90]{9545fig8.eps}\end{figure}$	Figure 8: ¹²CO(1-0) contours as in Fig. 6 ( left panel) superposed on the greyscale ¹²CO(2-1) map that has been tapered, convolved to the same resolution, and corrected for primary beam attenuation, in units of ${\rm Jy~beam^{-1}~km~s}^{-1}$ . The beam is plotted at lower left.
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$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90]{9545fig9.eps}\end{figure}$	Figure 9: Contours and greyscale of the CO(2-1)/CO(1-0) ratio map. Contours run from 0.1 to 1.8 in steps of 0.1 in temperature units.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9545fg11.ps} \end{figure}$	Figure 11: ¹²CO(1-0) position-velocity (p-v) diagram along the major axis of NGC 3147 using the whole velocity range +/-240 km s^-1. The coordinates of the center (0, 0), the heliocentric velocity, and PA used are given in Table 1. Contour levels are from 3.2 to $32~{\rm mJy~beam^{-1}}$ in steps of $3.2~{\rm mJy~beam^{-1}}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm]{9545fg12.ps} \end{figure}$	Figure 12: ¹²CO(1-0) position-velocity (p-v) diagram along the minor axis of NGC 3147 using the same velocity range, center, PA, and systemic velocity as for Fig. 11. Contour levels are from 2.8 to $28~{\rm mJy~beam^{-1}}$ in steps of $2.8~{\rm mJy~beam^{-1}}$ .
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f13c.eps} \end{figure}$	Figure 13: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the near-infrared J image from the CFHT, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f14c.eps} \end{figure}$	Figure 14: The J-K image from the CFHT with ¹²CO(2-1) integrated intensity overlaid in contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). North is up and east to the left.
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f15c.eps} \end{figure}$	Figure 15: GALEX FUV sky subtracted image of NGC 3147. The central 120 $^{\prime \prime }$ of the galaxy are shown. The box shows the central 50 $^{\prime \prime }$ , field of view of our ¹²CO observations.
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f16c.eps} \end{figure}$	Figure 16: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the GALEX FUV image of NGC 3147, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f17c.eps}\end{figure}$	Figure 17: Spitzer/IRAC ``dust-only'' image at 8 $\mu$ m of NGC 3147. The central 120 $^{\prime \prime }$ of the galaxy are shown. The box shows the central 50 $^{\prime \prime }$ , field of view of our ¹²CO observations.
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$\begin{figure} \par\includegraphics[width=8cm,angle=-90]{9545f18b.eps}\end{figure}$	Figure 18: Left panel: ¹²CO(1-0) contours (0.6 to 2.6 by 0.35 Jy km s^-1 beam^-1) superposed on the 8 $\mu$ m ``dust-only'' (Spitzer/IRAC) image of NGC 3147, shown in logarithmic levels. The central 50 $^{\prime \prime }$ are shown. Right panel: same for ¹²CO(2-1) contours (1.0 to 3.5 by 0.5 Jy km s^-1 beam^-1). The central 30 $^{\prime \prime }$ are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{9545f19.ps} \end{figure}$	Figure 19: Strengths (Q₁, Q₂, and total $Q_{\rm T}$ ) and phases ( $\phi _1$ and $\phi _2$ ) of the m=1 and m=2 Fourier components of the stellar potential inside a field of 48 $^{\prime \prime }$ in diameter (r < 4.6 kpc).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,bb=80 80 530 610]{9545f21.ps} \end{figure}$	Figure 21: Same as Fig. 20 for the ¹²CO(2-1) emission taken as a tracer of gas surface density.
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$\begin{figure} \par\includegraphics[angle=-90,width=18cm]{9545f22.ps} \end{figure}$	Figure 22: The torque, or more precisely the fraction of the angular momentum transferred from/to the gas in one rotation - dL/L - is plotted for ¹²CO(1-0) ( left) and ¹²CO(2-1) ( right).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{9545f23.ps} \end{figure}$	Figure 23: Model rotation curve and derived frequencies $\Omega$ , $\Omega -\kappa /2$ , and $\Omega +\kappa /2$ , for NGC 3147. The star symbols are the data derived from the CO kinematics, deprojected with an inclination of $i = 29.5^\circ$ . The horizontal line corresponds to $\Omega_{\rm p}~=~125$ km s^-1 kpc^-1.
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