Detalles de publicación
PP 013052
Hα kinematics of 11 starburst galaxies selected from the Sloan Digital Sky Survey
1Stockholm Observatory, Department of Astronomy, Stockholm University, AlbaNova Center, 106 91 Stockholm, Sweden
1Stockholm University Observatory, Sweden.
2.Oskar Klein Center for Cosmoparticle Physics, University of Stockholm, Sweden
3Instituto de Astrofísica de Canarias,4. Consjeo Superior de Investigaciones Científicas. 5. Departamento de Astrofísica, Universidad de La Laguna, 6. Instituto de Astrofísica de Andalucía
We present analysis of Fabry-Perot interferometric observations for a sample of 11 starburst galaxies with redshift z . 0.03 selected from the Sloan Digital Sky Survey. We have targeted the Hα λ6562.78 emission line at spatial sampling of
0.′′2 − 0.′′4 and at spectral resolution of R ∼ 16000. Studying two-dimensional maps for the velocity,velocity dispersion, line emission and continuum deliver new insights into the nature of starburst and postburst galaxies. The velocity fields are fitted to an exponential disc model, providing scale lengths and masses, to be compared with the photometric scale length and the mass estimated from the velocity dispersions. From the line emission the star formation rates are also calculated and compared with values in the literature.
We have found that between 55% and 64% of our sample show large scale dominating
rotation, while 27% show local rotation typically restricted to the central part of each system. The morphology and line profiles in the centre of eight objects are consistent with a recent merger, while another two seem to be involved in an accretion process which, for the moment, has not disrupted their kinematics.
0.′′2 − 0.′′4 and at spectral resolution of R ∼ 16000. Studying two-dimensional maps for the velocity,velocity dispersion, line emission and continuum deliver new insights into the nature of starburst and postburst galaxies. The velocity fields are fitted to an exponential disc model, providing scale lengths and masses, to be compared with the photometric scale length and the mass estimated from the velocity dispersions. From the line emission the star formation rates are also calculated and compared with values in the literature.
We have found that between 55% and 64% of our sample show large scale dominating
rotation, while 27% show local rotation typically restricted to the central part of each system. The morphology and line profiles in the centre of eight objects are consistent with a recent merger, while another two seem to be involved in an accretion process which, for the moment, has not disrupted their kinematics.