Hα and FUV luminosities from a stochastically formed stellar population
Abstract
It has been observed that the ratio of Hα to FUV luminosity (L Hα/L FUV ) 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 (L Hα/L FUV ). We present a model for the total L Hα and L FUV luminosity arising from a randomly populated IMF following the Salpeter power law and the clustering law of Oey & Clarke (2007).
- Publication:
-
The Spectral Energy Distribution of Galaxies - SED 2011
- Pub Date:
- August 2012
- DOI:
- 10.1017/S1743921312008721
- Bibcode:
- 2012IAUS..284...53N
- Keywords:
-
- methods: numerical;
- stars: mass function;
- galaxies: star clusters