Volume 374, Number 3, August II 2001
|Page(s)||800 - 823|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 August 2001|
Dynamics of blue compact galaxies, as revealed by their Hα velocity fields*
II. Mass models and the starburst triggering mechanism
SCFAB, Stockholm Observatory, Department of Astronomy, 106 91 Stockholm, Sweden
2 Laboratoire d'Astrophysique de Marseille, Observatoire de Marseille, 2 place le Verrier, 13248 Marseille Cedex 04, France
3 Astronomiska observatoriet, Box 515, 75120 Uppsala, Sweden
4 Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain
Corresponding author: G. Östlin, email@example.com
Accepted: 17 May 2001
The Hα velocity fields of a sample of six luminous blue compact galaxies (BCGs) and two companions have been obtained by observations with a scanning Fabry-Perot interferometer. The Fabry-Perot images, velocity fields and rotations curves have been presented in a previous paper (Paper I). In general, the velocity fields are irregular and often contain secondary dynamical components, but display overall rotation. The two companions have more regular velocity fields and rotation curves. In this article we analyse the velocity fields and dynamics together with the morphology of the studied BCGs, and present detailed mass models. In addition, we model the stellar mass content by means of multicolour surface photometry and spectral evolutionary synthesis analysis. By comparison of the masses of stars and those derived from the rotation curve, we show that about half of the galaxies cannot be supported by rotation alone. The morphology and dynamics of the BCGs suggest that the starburst activity in these galaxies are most likely triggered by mergers involving gas-rich dwarf galaxies and/or massive gas clouds.
Key words: galaxies: compact / galaxies: starburst / galaxies: kinematics and dynamics / galaxies: evolution / galaxies: formation / galaxies: interactions
© ESO, 2001
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