Issue |
A&A
Volume 379, Number 2, November IV 2001
|
|
---|---|---|
Page(s) | 347 - 361 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20011242 | |
Published online | 15 November 2001 |
VLA HI Imaging of the brightest spiral galaxies in Coma*
II. The HI Atlas and deep continuum imaging of selected early type galaxies
1
Departamento de Astronomía, Universidad de Guanajuato. Apdo. Postal 144, Guanajuato 36000, México
2
Observatoire de Paris DAEC, and UMR 8631, associé au CNRS et à l'Université Paris 7, 92195 Meudon Cedex, France
3
Department of Astronomy, Columbia University, 550 W 120th Street, New York, NY 10027, USA
Corresponding author: H. Bravo-Alfaro, hector@astro.ugto.mx
Received:
11
July
2001
Accepted:
4
September
2001
In the first paper of this series we used Hi observations of the 19
brightest spirals in Coma to analyze the dynamical state of the cluster. In
this paper we present the detailed Hi distribution and kinematics of the
spirals that were detected in Hi, and radio continuum data for a sample of
star forming and post starburst galaxies in Coma. We discuss the importance
of ICM-ISM interactions to explain the observed Hi morphology. A rough
comparison of observed Hi sizes with predicted Hi sizes from simulations by
Abadi et al. ([CITE]) gives reasonable agreement. We use the results on radio
continuum emission to estimate the star formation rate in the PSB galaxies we
pointed at. The radio continuum emission in the 11 so called post starburst
galaxies, identified by Caldwell et al. ([CITE]) in the cluster, is
weak. Eight of the 11 were not detected down to a 3 sigma upper limit of
0.6 mJy. This sets an upper limit to the star formation rate in these
galaxies of less than 0.2 yr-1. The three detected post
starburst galaxies have a star formation rate of less than one solar
mass per year. Thus none of the post starburst galaxies in Coma are dust
enshrouded starbursts.
Key words: galaxies: clusters: individual: Coma / radio lines: galaxies
© ESO, 2001
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