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The Wolf-Rayet population in the galaxy CTS 1026

Published online by Cambridge University Press:  26 May 2016

Götz Gräfener ,
Lars Koesterke  and
Wolf-Rainer Hamann
Götz Gräfener
Affiliation:
Lehrstuhl Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, BRD Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Lars Koesterke
Affiliation:
Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Wolf-Rainer Hamann
Affiliation:
Lehrstuhl Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, BRD

Abstract

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The blue compact H ii galaxy CTS 1026 shows very strong WR emission features (Wλ(4680) = 17 Å and Wλ(5800) = 10 Å). We present high s/n optical spectra of the nucleus of this object, augmented by IUE UV spectra. By analysis of the WR profile shapes, we determine the dominant spectral types and the number of WN and WC stars in the star forming region. The number of O-type stars is determined by comparing the observed UV to optical flux distribution to population synthesis models.

Type
Part 4. Feedback from Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 714 - 715
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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