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Star-Forming Regions in the SMC

Published online by Cambridge University Press:  01 August 2006

I. Gonidakis
Affiliation:
Dpt. of Astrophysics, Astronomy & Mechanics, Univ. of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
E. Livanou
Affiliation:
Dpt. of Astrophysics, Astronomy & Mechanics, Univ. of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
E. Kontizas
Affiliation:
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
M. Kontizas
Affiliation:
Dpt. of Astrophysics, Astronomy & Mechanics, Univ. of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
D. Kester
Affiliation:
SRON, Netherlands Inst. for Space Research, P.O. Box 800, 9700 AV Groningen, Netherlands
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
P. Tsalmantza
Affiliation:
Dpt. of Astrophysics, Astronomy & Mechanics, Univ. of Athens, GR-15783 Athens, Greece email: elivanou@phys.uoa.gr
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Abstract

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SMC has been going through an active star formation epoch, especially during the last 0.2 Gyr when the close encounter with the LMC occured. Our goal is to detect regions dominated by early-type stars and gas and examine their behaviour at different wavelengths. Spectral energy distributions, a colour-magnitude diagram and a two-colour diagram from IRAS data (Bontekoe, Koperet & Kester (1994); Bontekoe, Kester, Stanimirović, et al. (1999)) for these regions were used in order to compare their properties with those of starburst galaxies (Helou (1986); Lehnert & Heckman (1995)). We have selected 50 stellar complexes with increased 100-μm IRAS flux, with detetected emission in all IRAS bands and/or high concentration of young stars. Ranking them by size (Maragoudaki, Kontizas, Kontizas, et al. (1998)), a total of what we call 24 aggregates, 23 complexes and 3 super-complexes were found. Radio continuum maps at 8.6-GHz (Haynes, Murray, Klein, et al. (1986)) and the CO (1→0) line (Mizuno, Rubio, Mizuno, et al. (2001)) were also correlated with the map of the complexes. Only 8 of them show enhanced star formation activity according to their IR properties and 8.6-GHz map, however, none of them resembles the IR behaviour of starburst regions found in the LMC and starburst galaxies (Livanou, Kontizas, Gonidakis, et al. (2006)). The south-west part of the “bar” has the most diverse intensity of star formation, with CO emission coincident with the largest structure. In the north-eastern end of the “bar”, star formation is likely to have commenced in the recent past, with molecular gas being abundant in this region. Ongoing and future star formation are revealed in the wing, while it appears to have ceased in the central “bar”.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

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