All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{4745fig1.ps} \end{figure}$ Figure 1: Map of the central spectra taken towards NGC 1275. Each spectrum has a velocity scale from -600 to 600 km s^-1, and a temperature scale in $T_{\rm A}^*$ from -10 to 40 mK. The positional scale shows RA-Dec in arcsec, centered on the 3C 84 radio source.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4745f2.eps}\hspace*{6mm} \includegraphics[width=6.2cm,height=10.5cm,clip]{4745fig2.ps} \end{figure}$ Figure 2: Left side: integrated emission in CO(2-1) over the whole map. The region covered by the HERA observations is a central $138\times 138\hbox {$^{\prime \prime }$ }$ region, with a northern $66\times 66\hbox {$^{\prime \prime }$ }$ additional region centered at (0, 108 $^{\prime \prime }$ ) to cover the vertical northern filaments. Contours are linear, from 10 to 100% of the maximum emission of 8.3 K km s^-1, in $T_{\rm A}^*$ scale. The beam of 12 $^{\prime \prime }$ is indicated at the bottom left. Right side: H $\alpha$ image with the same scale (Conselice et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4745fig3.ps}\hspace*{3mm} \includegraphics[angle=-90,width=7.6cm,clip]{4745fig4.ps} \end{figure}$ Figure 3: Left side: positions of selected CO(2-1) spectra (in black) together with the H $\alpha$ regions (in circles) observed by Conselice et al. (2001). Black numbers refer to regions described in Table 3. Circled red numbers refer to positions of Conselice's Fig. 5 regions. Right side: the brightest CO(2-1) spectra along the H $\alpha$ filaments.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{4745fig5.ps} \end{figure}$ Figure 4: Cold molecular gas mass evaluated from each fitted CO(2-1) line versus radius. The mean mass per point at each radius is overlaid using a dashed line. The continuous line represents the total accumulated mass at radius ${\le }r$ . Also shown are previous measurements with the author name.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4745fig6.ps} \end{figure}$ Figure 5: Isovelocity map of the CO(2-1) emission. The contours are from -100 to 80 km s^-1, increasing in steps of 20 km s^-1. The beam of 12 $\hbox {$^{\prime \prime }$ }$ is indicated at the bottom left. Negative velocities are shown as dashed contours.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{4745f6.eps} \end{figure}$ Figure 6: Average of the selected spectra plotted in Fig. 3 ( $T_{\rm A}$ (K) vs. Velocity). Overlaid are 2 Gaussian profiles with positions 292.6 km s^-1 and -51.3 km s^-1, and widths 226 km s^-1 and 286 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{4745fig8.ps}\includegraphics[angle=-90,width=6.1cm,clip]{4745fig9.ps} \end{figure}$ Figure 7: Left side: CO(2-1) velocities versus radius plotted in black. H $\alpha$ velocity distribution from Conselice et al. (2001) plotted in purple. Overlaid in red, the rotation curve expected for gas bounded in a galactic potential created by a bulge ( $M_{\rm bulge} = 3 \times 10^{10}$ $M_\odot$ , $r_{\rm bulge} = 0.6$ kpc), a disk ( $M_{\rm disk} = 1.4 \times 10^{11}$ $M_\odot$ , $r_{\rm disk} = 3.5$ kpc), a Black Hole ( $M_{\rm BH} = 4 \times 10^{8}$ $M_\odot$ ) and a Dark matter Halo ( $M_{\rm DM} = 5 \times 10^{11}$ $M_\odot$ in $r_{\rm DM} = 42$ kpc, with then $M(r) \propto r^2$ ). Right side: comparison of the CO(2-1) velocity with the H $\alpha$ filament velocity in the central region of Perseus.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{4745fig10.ps} \end{figure}$ Figure 8: CO(2-1) line width radial distribution. Plotted in blue is the escape velocity computed from the mass distribution shown in Fig. 7. Plotted in red is $V_{\rm crit} = 3.36$ G $\Sigma$ / $\kappa$ , the Toomre lower limit of the velocity dispersion for a rotating gas disk with $\Sigma = 500$ $M_\odot$ pc^-2 to ensure gas stability.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{4745fig11.ps} \end{figure}$ Figure 9: Cold molecular gas mass as a function of H $\alpha$ luminosity for the regions in the filaments detected at both wavelengths (see Table 3). Circles are CO detections from Edge et al. (2001), squares are CO detections from Salomé & Combes (2004a) and triangles are present results. Overlaid in dashed line is the linear relation fitted by Salomé & Combes (2003). Added in continuous line is a better relation which include low mass regions detected in NGC 1275 which also follow this relation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4745fig12.ps} \end{figure}$ Figure 10: Normalized CO(2-1) intensity (Ico in K km s^-1) of selected spectra vs. radius together with normalized H $\alpha$ (erg cm^-2 s^-1) flux from Conselice et al. (2001), cf Fig. 3. Overlaid is a grid of $\propto$ r^-2 curves.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4745fig13.ps} \end{figure}$ Figure 11: Contours of the CO(2-1) emission (black) superimposed on the X-ray image (false colours, indicating intensity) by Fabian et al. (2003), and with the radio contours (white) by Pedlar et al. (1990). The relativistic plasma ejected by the central AGN in the two radio lobes pushes out the X-ray gas, which is compressed on the rims, and cools down there. The CO is also found at the border of the northern cavity.
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In the text

$\begin{figure} \par\begin{tabular}{cc} \includegraphics[width=2cm, angle=-90]{4... ...\includegraphics[width=2cm, angle=-90]{4745fig22.ps}\end{tabular}\end{figure}$ Figure 12: Eight CO(2-1) spectra extracted from regions corresponding to the Shields and Filippenko star cluster region. The last spectrum at the bottom right is a line fitting the mean emission over the 8 regions displayed here. When averaging all these spectra, two distinct components can be distinguished separated by $\sim$ 260 km s^-1, a broad line and a narrow line which could be coming from the filament and the star cluster region respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{4745fig1.ps} \end{figure}$	Figure 1: Map of the central spectra taken towards NGC 1275. Each spectrum has a velocity scale from -600 to 600 km s^-1, and a temperature scale in $T_{\rm A}^*$ from -10 to 40 mK. The positional scale shows RA-Dec in arcsec, centered on the 3C 84 radio source.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4745fig3.ps}\hspace*{3mm} \includegraphics[angle=-90,width=7.6cm,clip]{4745fig4.ps} \end{figure}$	Figure 3: Left side: positions of selected CO(2-1) spectra (in black) together with the H $\alpha$ regions (in circles) observed by Conselice et al. (2001). Black numbers refer to regions described in Table 3. Circled red numbers refer to positions of Conselice's Fig. 5 regions. Right side: the brightest CO(2-1) spectra along the H $\alpha$ filaments.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{4745fig5.ps} \end{figure}$	Figure 4: Cold molecular gas mass evaluated from each fitted CO(2-1) line versus radius. The mean mass per point at each radius is overlaid using a dashed line. The continuous line represents the total accumulated mass at radius ${\le }r$ . Also shown are previous measurements with the author name.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4745fig6.ps} \end{figure}$	Figure 5: Isovelocity map of the CO(2-1) emission. The contours are from -100 to 80 km s^-1, increasing in steps of 20 km s^-1. The beam of 12 $\hbox {$^{\prime \prime }$ }$ is indicated at the bottom left. Negative velocities are shown as dashed contours.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{4745f6.eps} \end{figure}$	Figure 6: Average of the selected spectra plotted in Fig. 3 ( $T_{\rm A}$ (K) vs. Velocity). Overlaid are 2 Gaussian profiles with positions 292.6 km s^-1 and -51.3 km s^-1, and widths 226 km s^-1 and 286 km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{4745fig10.ps} \end{figure}$	Figure 8: CO(2-1) line width radial distribution. Plotted in blue is the escape velocity computed from the mass distribution shown in Fig. 7. Plotted in red is $V_{\rm crit} = 3.36$ G $\Sigma$ / $\kappa$ , the Toomre lower limit of the velocity dispersion for a rotating gas disk with $\Sigma = 500$ $M_\odot$ pc^-2 to ensure gas stability.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4745fig12.ps} \end{figure}$	Figure 10: Normalized CO(2-1) intensity (Ico in K km s^-1) of selected spectra vs. radius together with normalized H $\alpha$ (erg cm^-2 s^-1) flux from Conselice et al. (2001), cf Fig. 3. Overlaid is a grid of $\propto$ r^-2 curves.
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