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Star-Burst Regions in the LMC

Published online by Cambridge University Press:  01 August 2006

E. Livanou ,
M. Kontizas ,
I. Gonidakis ,
E. Kontizas ,
U. Klein ,
Y. Fukui  and
N. Mizuno
E. Livanou
Affiliation:
Department of Astrophysics, Astronomy & Mechanics, Faculty of Physics, University of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
M. Kontizas
Affiliation:
Department of Astrophysics, Astronomy & Mechanics, Faculty of Physics, University of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
I. Gonidakis
Affiliation:
Department of Astrophysics, Astronomy & Mechanics, Faculty of Physics, University of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
E. Kontizas
Affiliation:
Institute for Astronomy and Astrophysics, National Observatory of Athens, P.O. Box 20048, GR-11810 Athens, Greece
U. Klein
Affiliation:
Radioastronomisches Inst.der Universität, Bonn, Auf dem Hugel 71, 53121 Bonn, Germany
Y. Fukui
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan
N. Mizuno
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan
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Abstract

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Filamentary structures of early type stars are found to be a common feature of the MCs formed ~0.9 − 2 × 108yr ago. As we go to younger ages these large structures appear fragmented and sooner or later form young clusters and associations. In the optical domain we have detected 56 such large structures of young objects, known as stellar complexes in the LMC (Maragoudaki, Kontizas, Kontizas, et al. (1998)) and investigate their properties. IRAS data of the LMC stellar complexes were compared with observations of starburst galaxies (Helou (1986); Lehnert & Heckman (1996)). It has been found that nearly 1/4 of the stellar complexes are extremely active resembling the IR behaviour of starburst galaxies and HII regions. These stellar complexes are called here “starburst regions”. They host an increased number of HII regions, SNRs, stellar associations and nebulae. The main starburst tracers are their IR luminosity F60 and the 8.6-GHz radio emission (8.6-GHz data: Dickel, McIntire, Gruendl, et al. (2005)). In Table 1 the characteristics of the various types of complexes are given. Finally the evolution of all stellar complexes is discussed based on the CO emission (CO data: Fukui, Mizuno, Yamagushi, et al. (1999)). More than 50% of the starburst and starburst candidate regions show enhanced CO emission, indicating ongoing and future evolution.

Keywords

galaxies: structureMagellanic Cloudsstars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 318
Copyright
Copyright © International Astronomical Union 2007

References

Dickel, J.R., McIntire, V.J., Gruendl, R.A., & Milne, D.K. 2005, ApJ L29, 790.CrossRefGoogle Scholar
Fukui, Y., Mizuno, N., Yamagushi, R. 1999, PASJ 51, 745.CrossRefGoogle Scholar
Helou, G. 1986, ApJ 311, L33.CrossRefGoogle Scholar
Lehnert, M.D. & Heckman, T.M. 1996, ApJ 472, 546.Google Scholar
Maragoudaki, F., Kontizas, M., Kontizas, E., Dapergolas, A., & Morgan, D.H. 1998, A&A 338, 29.Google Scholar