Abstract
The so called ‘empirical methods’ for the determination of nebular abundances are imperative when dealing with the many objects where the detection of weak temperature sensitive lines is not possible (ionized regions of low excitation including many galactic nuclei, HII regions in distant galaxies, low surface brightness objects etc. ...). Probably the observable most widely used is R23 (Pagel et al., 1979). Photoionization models show however that it depends both on ionization parameter and stellar effective temperature and different assumptions about the effects of metallicity on either nebular ionization structure or ionizing temperature have to be made to properly calibrate it at high metallicities.
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References
Pagel, B.E.J., Edmunds, M.G., Blackwell, D.E., Chun, M.S. and Smith, G.: 1979, MNRAS 189, 95.
Vílchez, J.M. and Esteban, C.: 1996, MNRAS 280, 720.
Díaz, A.I and Pérez-Montero. E.: 2000, MNRAS 312, 130.
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© 2001 Springer Science+Business Media Dordrecht
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Díaz, A.I., Pérez-Montero, E. (2001). Empirical Abundance Determination for Ionized Nebulae. In: Vílchez, J.M., Stasińska, G., Pérez, E. (eds) The Evolution of Galaxies. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-3313-7_43
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DOI: https://doi.org/10.1007/978-94-017-3313-7_43
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