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Hα and FUV luminosities from a stochastically formed stellar population

Published online by Cambridge University Press:  17 August 2012

Nidia Lugo Lopez L. ,
Gladis Magris C.  and
Antonio Parravano
Nidia Lugo Lopez L.
Affiliation:
Universidad de los Andes email: nlugo@cida.ve, parravan@ula.ve Centro de Investigaciones de Astronomía (CIDA), Apdo. Postal 264, 5101-A, Mérida, Venezuela email: magris@cida.ve
Gladis Magris C.
Affiliation:
Centro de Investigaciones de Astronomía (CIDA), Apdo. Postal 264, 5101-A, Mérida, Venezuela email: magris@cida.ve
Antonio Parravano
Affiliation:
Universidad de los Andes email: nlugo@cida.ve, parravan@ula.ve
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Abstract

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It has been observed that the ratio of Hα to FUV luminosity (LHα/LFUV) is lower in low surface brightness galaxies. This behaviour has been attributed to systematic variations of the upper mass end and/or the slope of the Initial Mass Function (IMF) Meurer et al. (2009) and Lee et al. (2009)). However these hypotheses do not explain the observed scatter in luminosity ratio (LHα/LFUV). We present a model for the total LHα and LFUV luminosity arising from a randomly populated IMF following the Salpeter power law and the clustering law of Oey & Clarke (2007).

Keywords

methods: numericalstars: mass functiongalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 53 - 55
Copyright
Copyright © International Astronomical Union 2012

References

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