Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004 , 18080 Granada, Spain
2 Institut d'Astrophysique de Paris, CNRS, 98bis Bd Arago, 75014 Paris, France
3 Departamento de Astronomía, Universidad de Chile, Casilla 36D, Santiago, Chile
4 Observatories of the Carnegie Institution of Washington, 813 Barbara Street, Pasadena, CA91101, USA
Corresponding author: I. Márquez, email@example.com
Accepted: 18 November 2003
We present the kinematical data obtained for a sample of active (Seyfert) and non active isolated spiral galaxies, based on long slit spectra along several position angles in the Hα line region and, in some cases, in the Ca triplet region as well. Gas velocity distributions are presented, together with a simple circular rotation model that allows us to determine the kinematical major axes. Stellar velocity distributions are also shown. The main result is that active and control galaxies seem to be equivalent in all kinematical aspects. For both subsamples, the departure from pure circular rotation in some galaxies can be explained by the presence of a bar and/or of a spiral arm. They also present the same kind of peculiarities, in particular, S-shape structures are quite common near the nuclear regions. They define very similar Tully-Fisher relations. Emission line ratios are given for all the detected HII regions; the analysis of the [NII]/Hα metallicity indicator shows that active and non-active galaxies have indistinguishable disk metallicities. These results argue in favour of active and non-active isolated spiral galaxies having essentially the same properties, in agreement with our previous results based on the analysis of near infrared images. It appears now necessary to confirm these results on a larger sample.
Key words: galaxies: spiral / galaxies: kinematics and dynamics / galaxies: structure / galaxies: interactions
Based on observations made with WHT operated on the island of La Palma by ING in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias, the European Southern Observatory (La Silla), Calar Alto Observatory (Almería, Spain) and Las Campanas Observatories (Chile).
Table 3 and Figs. [see full text], 5, 7, 9, 11, 13, 15, 17, 19, 21, 23, 25, 28, 30, 32, 34, 36, 38, 40, 42, 44, 46, 48, 50 and 52 are only available in electronic form at http://www.edpsciences.org
© ESO, 2004