Hostname: page-component-8448b6f56d-t5pn6 Total loading time: 0 Render date: 2024-04-17T15:25:47.906Z Has data issue: false hasContentIssue false
  • English
  • Français

Nebular abundances in galaxies: Beware of biases

Published online by Cambridge University Press:  13 April 2010

Grażyna Stasińska
Grażyna Stasińska*
Affiliation:
LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; Place Jules Janssen 92190 Meudon, France email: grazyna.stasinska@obspm.fr
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The derivation of nebular abundances in galaxies using strong line methods is simple and quick. Various indices have been designed and calibrated for this purpose, and they are widely used. However, abundances derived with such methods may be significantly biased, if the objects under study have different structural properties (hardness of the ionizing radiation field, morphology of the nebulae) than those used to calibrate the methods. Special caution is required when comparing the metallicities of different samples, like, for example, blue compact galaxies and other emission line dwarf galaxies, or samples at different redshifts.

Keywords

galaxies: abundancesHII regions
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 93 - 96
Copyright
Copyright © International Astronomical Union 2010

References

Adelman-McCarthy, J. K. et al. 2008, ApJS, 175, 297CrossRefGoogle Scholar
Alloin, D., Collin-Souffrin, S., Joly, M., & Vigroux, L. 1979, A&A 78, 200Google Scholar
Dopita, M. A. et al. 2006, ApJ, 647, 244CrossRefGoogle Scholar
Izotov, Y. I., Stasińska, G., Meynet, G. et al. 2006, A&A, 448, 955Google Scholar
Kewley, L. J. & Ellison, S. L. 2008, ApJ, 681, 1183CrossRefGoogle Scholar
McGaugh, S. S. 1991, ApJ, 380, 140CrossRefGoogle Scholar
Nagao, T., Maiolino, R., & Marconi, A. 2006, A&A, 459, 85Google Scholar
Pérez-Montero, E. & Díaz, A. I. 2005, MNRAS, 361, 1063CrossRefGoogle Scholar
Pagel, B. E. J., Edmunds, M. G., Blackwell, D. E. et al. 1979, MNRAS, 189, 95CrossRefGoogle Scholar
Sánchez Almeida, J., Aguerri, J. A. L., Muñoz-Tuñón, C., & Vazdekis, A. 2009, ApJ, 698, 1497CrossRefGoogle Scholar
Sánchez Almeida, J., Muñoz-Tuñón, C., Amorín, R., Aguerri, J. A., Sánchez-Janssen, R., & Tenorio-Tagle, G. 2008, ApJ, 685, 194CrossRefGoogle Scholar
Stasińska, G. 2004, cmpe.conf, 115CrossRefGoogle Scholar
Stasińska, G. 2006, A&A, 454, L127Google Scholar
Stasińska, G. 2008, IAUS, 255, 375CrossRefGoogle Scholar
Storchi-Bergmann, T., Calzetti, D., & Kinney, A. L., 1994, ApJ, 429, 572CrossRefGoogle Scholar
Vale Asari, N., Stasińska, G., Cid Fernandes, R., Gomes, J. M., Schlickmann, M., Mateus, A., & Schoenell, W. 2009, MNRAS, 396, L71CrossRefGoogle Scholar
Vilchez, J. M. & Esteban, C. 1996, MNRAS, 280, 720CrossRefGoogle Scholar