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Photo-ionization models of NGC 2363 and their implications

Published online by Cambridge University Press:  25 May 2016

Valentina Luridiana ,
Manuel Peimbert  and
Claus Leitherer
Valentina Luridiana
Affiliation:
Instituto de Astronomía, UNAM, Mexico
Manuel Peimbert
Affiliation:
Instituto de Astronomía, UNAM, Mexico
Claus Leitherer
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA.

Abstract

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We compute photo-ionization models for the giant extragalactic H II region NGC 2363, and compare them with optical observational data. We focus on the following observational constraints: F(Hβ), Ne, EW(Hβ), and the ratios of I(λ 5007), I(λ 4363), I(λ 3727), I(λ 6300), I(λ 6720) and I(λ 4686) relative to I(Hβ). We discuss the variations of the emission spectra obtained with different input parameters. We show that low metallicity models (Z = 0.10Z⊙) cannot reproduce the observed features of the spectrum, and that the disagreement can be satisfactorily overcome by allowing for spatial temperature fluctuations in the nebula. Accordingly, we show that the metallicity of NGC 2363 has most probably been underestimated, and that a value of Z ≃ 0.25 Z⊙ is in better agreement with the observational data than the usually adopted value Z≃0.10Z⊙. We also derive values for the slope and the high mass end of the IMF, as well as the age of the stellar cluster.

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. 487 - 488
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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