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Star formation in NGC 3603

Published online by Cambridge University Press:  25 May 2016

Mauricio Tapia  and
Brenda Pérez
Mauricio Tapia
Affiliation:
Instituto de Astronomía, UNAM, Ensenada, B.C., Mexico
Brenda Pérez
Affiliation:
Instituto de Astronomía, UNAM, Ensenada, B.C., Mexico

Extract

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NGC 3603 is the most massive optically visible H II region in our Galaxy and is considered to be the Galactic analogue to 30 Doradus and, thus, a prototype of the starburst phenomenon. Its core, known as WR 43 (HD 97950), contains several dozens of O-B0 stars within 35″. These have been studied with very high resolution in the optical and near-IR. Melnick, Tapia & Terlevich (1989) concluded that the starburst cluster has an age spread of 1 to 2 Myr and that its boundaries extend to ∼60″, while Eisenhauer et al. (1998) determined that the lower mass stars in the core are younger than 1 Myr.

Type
Part 4. Wolf-Rayet stars and other hot massive stars in the Galactic Center and in Local Group giant H II regions (individual stars)
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 499 - 500
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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Frogel, J.A., Persson, S.E., Aaronson, M. 1977, ApJ 213, 723 Google Scholar
Melnick, J., Tapia, M., Terlevich, R. 1989, A&A 213, 89 Google Scholar
Persi, P., Tapia, M., Roth, M., Ferrari-Toniolo, M. 1985, A&A 144, 275 Google Scholar
Roth, M. et al. 1986, in: Peimbert, M. & Jugaku, J. (eds.), Star Forming Regions, Proc. IAU Symp. No. 115 (Dordrecht: Reidel), p. 182 Google Scholar
Rubio, M., Barbá, R.H, Walborn, N.R., Probst, R.G., Garcia, J., Roth, M.R. 1998, AJ 116, 1708 Google Scholar
Tapia, M. 1981, PhD Thesis, University of Edinburgh Google Scholar