Astronomy & Astrophysics

Free access article

Issue		A&A Volume 374, Number 2, August I 2001
Page(s)		394 - 411
Section		Extragalactic astronomy
DOI		10.1051/0004-6361:20010625

A&A 374, 394-411 (2001)
DOI: 10.1051/0004-6361:20010625

Kinematic properties of gas and stars in 20 disc galaxies

J. C. Vega Beltrán^{1, 2}, A. Pizzella³, E. M. Corsini³, J. G. Funes S. J.⁴, W. W. Zeilinger⁵, J. E. Beckman¹ and F. Bertola⁶

¹ Instituto Astrofísico de Canarias, Calle Via Lactea s/n, 38200 La Laguna, Spain
² Guest investigator of the UK Astronomy Data Centre
³ Osservatorio Astrofisico di Asiago, Dipartimento di Astronomia, Università di Padova, via dell'Osservatorio 8, 36012 Asiago, Italy
⁴ Vatican Observatory, University of Arizona, Tucson, AZ 85721, USA
⁵ Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria
⁶ Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy

(Received 21 December 2000 / Accepted 23 April 2001)

Abstract
Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion ( $V_{\rm g} > V_\star$ and $\sigma_{\rm g} <$ ß), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions ( $V_{\rm g} \simeq V_\star$ and $\sigma_{\rm g} \simeq$ ß). Incorporating the early-type disc galaxies studied by Bertola et al. (1995), Fisher (1997) and Corsini et al. (1999), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of ßmeasured at $R_{\rm e}/4$ turns out to be strongly correlated with the galaxy morphological type, while $\sigma_{\rm g}$ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.

Key words: galaxies: kinematics and dynamics -- galaxies: elliptical and lenticular, cD -- galaxies: spiral

Offprint request: J. C. Vega Beltrán, jvega@ll.iac.es

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