Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0108.f1}\end{figure}$ Figure 1: Tully-Fisher relation for the galaxies of our sample (pentagons for active galaxies and triangles for non-active ones), together with the isolated galaxies of the M111 sample (empty circles). M_B is the B corrected absolute magnitude, and $W_{{\rm max}}$ = 2 $\times$ $V_{{\rm max}}$ (km $\rm s^{-1}$ ) is the total amplitude of the rotation curve. The line indicates the TF relation by Tully & Pierce (2000).
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f2.eps}\end{figure}$ Figure 2: Velocity distributions for UGC 1395. As for all similar figures, gas velocities derived from H $\alpha$ and H $\beta$ are shown as black dots (with error bars) and empty light circles respectively. Stellar velocities are shown with stars. For PA = 35 and 80 $^\circ$ an enlarged part of the central region is plotted to see better the corresponding stellar kinematics. An asterisk after the PA indicates the slit position angle coinciding with the major axis. The line corresponds to the rotation model which best reproduces the data.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f4.eps}\end{figure}$ Figure 4: Velocity distributions for IC 184. The two sets of two curves along PA = 7 and PA = 97 correspond to the LC (left) and WHT (right) data. An enlarged part of the central zone is shown with stars indicating the stellar component.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f6}\end{figure}$ Figure 6: Velocity distributions for IC 1816.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f8.eps}\end{figure}$ Figure 8: Velocity distributions for UGC 3223. The two sets of curves along PA = 80 $^\circ$ and PA = 170 $^\circ$ correspond to 4m class telescopes (right) and ESO (left) data.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f10.eps}\end{figure}$ Figure 10: Velocity distributions for NGC 2639. The top right figure shows an enlargement of the central region with the stellar velocities indicated in blue.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f12.eps}\end{figure}$ Figure 12: Velocity distributions for IC 2510.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f14.eps}\end{figure}$ Figure 14: Velocity distributions for NGC 3660. The ESO96 (left) and WHT99 (right) curves are on the top line for PA = 115. A zoom of the central region of the WHT99 data along PA = 115 is shown in the second line, together with the curve along PA = 25 where a few velocities from the H $\beta$ line are visible in the very center. The ESO96 (left) and WHT99 (right) curves are on the third line for PA = 85. A zoom of the central region of the WHT00 data along PA = 85 is shown in the fourth line.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f16}\end{figure}$ Figure 16: Velocity distributions for NGC 4507.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f18}\end{figure}$ Figure 18: Velocity distributions for NGC 4785.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f20}\end{figure}$ Figure 20: Velocity distributions for NGC 5347.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f22.eps}\end{figure}$ Figure 22: Velocity distributions for NGC 5728.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f24.eps}\end{figure}$ Figure 24: Velocity distributions for ESO 139-12.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f26.eps}\end{figure}$ Figure 26: Velocity distributions for NGC 6814. An enlargement of the central $\pm$ 15 arcsec is given for PA = 30 $^\circ$ with the stellar velocity distribution as stars.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f27.eps}\end{figure}$ Figure 27: Velocity distributions for NGC 6860.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f29.eps}\par\end{figure}$ Figure 29: Velocity distributions for NGC 6890.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f31.eps}\end{figure}$ Figure 31: Velocity distributions for NGC 151.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f33}\end{figure}$ Figure 33: Velocity distribution for NGC 1357.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f35.eps}\end{figure}$ Figure 35: Velocity distributions for IC 454. The two sets of curves along PA = 140 $^\circ$ and PA = 110 $^\circ$ correspond to ESO (left) and CAHA (right) data.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f37}\end{figure}$ Figure 37: Velocity distributions for NGC 3571.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f39}\end{figure}$ Figure 39: Velocity distributions for NGC 6012.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f41.eps}\end{figure}$ Figure 41: Velocity distributions for NGC 7328.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f43}\end{figure}$ Figure 43: Average velocity distribution for NGC 2712.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f45}\par\end{figure}$ Figure 45: Average velocity distribution for NGC 3835. The individual points correspond to the data on either side of the nucleus.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f47}\par\par\end{figure}$ Figure 47: Velocity distribution for NGC 4162.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f49}\par\par\end{figure}$ Figure 49: Velocity distribution for NGC 4290.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f51}\par\end{figure}$ Figure 51: Average velocity distribution for NGC 6155.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0108.f53}\end{figure}$ Figure 53: a. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å), except for NGC 2639 and NGC 5347 which are flux calibrated (in erg s^-1 cm^-2 Å^-1).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0108.f54}\addtocounter{figure}{-1} \end{figure}$ Figure 53: b. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0108.f55}\addtocounter{figure}{-1} \end{figure}$ Figure 53: c. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å).
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In the text

$\begin{figure} \includegraphics[origin=rb,angle=-90,width=8cm,clip]{0108.f56}\end{figure}$ Figure 54: [NII]/H $\alpha$ intensity ratio as a function of distance of HII region to the nucleus, normalized to r₂₅ for the DEGAS sample (with stars for active galaxies and filled circles for non-active objects) and for the isolated spirals in M111 (empty circles) having the same absolute magnitude distribution ( -22<M_B < -19) (see text).
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f3.eps}\end{figure}$ Figure 3: Residuals from the model for UGC 1395.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f5.eps}\end{figure}$ Figure 5: Residuals from the model for IC 184.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f7}\end{figure}$ Figure 7: Residuals from the model for IC 1816.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f9.eps}\end{figure}$ Figure 9: Residuals from the model for UGC 3223.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f11.eps}\end{figure}$ Figure 11: Residuals from the model for NGC 2639.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f13.eps}\end{figure}$ Figure 13: Residuals from the model for IC 2510.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f15.eps}\end{figure}$ Figure 15: Residuals from the model for NGC 3660.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f17}\end{figure}$ Figure 17: Residuals from the model for NGC 4507.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f19}\end{figure}$ Figure 19: Residuals from the model for NGC 4785.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f21}\end{figure}$ Figure 21: Residuals from the model for NGC 5347.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f23.eps}\end{figure}$ Figure 23: Residuals from the model for NGC 5728.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f25.eps}\end{figure}$ Figure 25: Residuals from the model for ESO 139-G12.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f28.eps}\end{figure}$ Figure 28: Residuals from the model for NGC 6860.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f30.eps}\end{figure}$ Figure 30: Residuals from the model for NGC 6890.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f32.eps}\end{figure}$ Figure 32: Residuals from the model for NGC 151.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f34}\end{figure}$ Figure 34: Residuals from the model for NGC 1357.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f36.eps}\end{figure}$ Figure 36: Residuals from the model for IC 454.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f38}\end{figure}$ Figure 38: Residuals from the model for NGC 3571.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f40}\end{figure}$ Figure 40: Residuals from the model for NGC 6012.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f42.eps}\end{figure}$ Figure 42: Residuals from the model for NGC 7328.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f44}\end{figure}$ Figure 44: Residuals from the model for NGC 2712.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f46}\end{figure}$ Figure 46: Residuals from the model for NGC 3835.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f48}\end{figure}$ Figure 48: Residuals from the model for NGC 4162.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f50}\end{figure}$ Figure 50: Residuals from the model for NGC 4290.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0108.f52}\end{figure}$ Figure 52: Residuals from the model for NGC 6155.
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In the text

$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f4.eps}\end{figure}$	Figure 4: Velocity distributions for IC 184. The two sets of two curves along PA = 7 and PA = 97 correspond to the LC (left) and WHT (right) data. An enlarged part of the central zone is shown with stars indicating the stellar component.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f6}\end{figure}$	Figure 6: Velocity distributions for IC 1816.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f8.eps}\end{figure}$	Figure 8: Velocity distributions for UGC 3223. The two sets of curves along PA = 80 $^\circ$ and PA = 170 $^\circ$ correspond to 4m class telescopes (right) and ESO (left) data.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f10.eps}\end{figure}$	Figure 10: Velocity distributions for NGC 2639. The top right figure shows an enlargement of the central region with the stellar velocities indicated in blue.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f12.eps}\end{figure}$	Figure 12: Velocity distributions for IC 2510.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f16}\end{figure}$	Figure 16: Velocity distributions for NGC 4507.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f18}\end{figure}$	Figure 18: Velocity distributions for NGC 4785.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f20}\end{figure}$	Figure 20: Velocity distributions for NGC 5347.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f22.eps}\end{figure}$	Figure 22: Velocity distributions for NGC 5728.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f24.eps}\end{figure}$	Figure 24: Velocity distributions for ESO 139-12.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f26.eps}\end{figure}$	Figure 26: Velocity distributions for NGC 6814. An enlargement of the central $\pm$ 15 arcsec is given for PA = 30 $^\circ$ with the stellar velocity distribution as stars.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f27.eps}\end{figure}$	Figure 27: Velocity distributions for NGC 6860.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f29.eps}\par\end{figure}$	Figure 29: Velocity distributions for NGC 6890.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f31.eps}\end{figure}$	Figure 31: Velocity distributions for NGC 151.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f33}\end{figure}$	Figure 33: Velocity distribution for NGC 1357.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{0108.f35.eps}\end{figure}$	Figure 35: Velocity distributions for IC 454. The two sets of curves along PA = 140 $^\circ$ and PA = 110 $^\circ$ correspond to ESO (left) and CAHA (right) data.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f37}\end{figure}$	Figure 37: Velocity distributions for NGC 3571.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f39}\end{figure}$	Figure 39: Velocity distributions for NGC 6012.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0108.f41.eps}\end{figure}$	Figure 41: Velocity distributions for NGC 7328.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f43}\end{figure}$	Figure 43: Average velocity distribution for NGC 2712.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0108.f45}\par\end{figure}$	Figure 45: Average velocity distribution for NGC 3835. The individual points correspond to the data on either side of the nucleus.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f47}\par\par\end{figure}$	Figure 47: Velocity distribution for NGC 4162.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f49}\par\par\end{figure}$	Figure 49: Velocity distribution for NGC 4290.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0108.f51}\par\end{figure}$	Figure 51: Average velocity distribution for NGC 6155.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0108.f53}\end{figure}$	Figure 53: a. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å), except for NGC 2639 and NGC 5347 which are flux calibrated (in erg s^-1 cm^-2 Å^-1).
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0108.f54}\addtocounter{figure}{-1} \end{figure}$	Figure 53: b. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å).
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0108.f55}\addtocounter{figure}{-1} \end{figure}$	Figure 53: c. Nuclear spectra, plotted as non calibrated flux vs. observed wavelength (in Å).
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$\begin{figure} \includegraphics[origin=rb,angle=-90,width=8cm,clip]{0108.f56}\end{figure}$	Figure 54: [NII]/H $\alpha$ intensity ratio as a function of distance of HII region to the nucleus, normalized to r₂₅ for the DEGAS sample (with stars for active galaxies and filled circles for non-active objects) and for the isolated spirals in M111 (empty circles) having the same absolute magnitude distribution ( -22<M_B < -19) (see text).
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$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f3.eps}\end{figure}$	Figure 3: Residuals from the model for UGC 1395.
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$\begin{figure} \par\includegraphics[width=15.9cm,clip]{0108.f5.eps}\end{figure}$	Figure 5: Residuals from the model for IC 184.
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