Abstract
AbstractThe UV capabilities of the GALEX satellite have revealed that there may be more star formation in low-density environments than previously recognized. Until GALEX, much of our understanding of star formation in the local universe had been based on observations of the Hα emission-line. A number of recent studies, however, have shown that the Hα luminosity appears to underestimate the star formation rate in dwarf and low surface brightness galaxies. Here, I summarize our work on this problem, which is based on a dwarf galaxy dominated sample of ∼ 300 late-type galaxies in the 11 Mpc Local Volume. The sample allows us to examine the discrepancy between Hα and UV SFRs using a statistical number of galaxies with activities less than 0.1 M⊙ yr−1. A range of potential causes are reviewed, and the possible impact of the discrepancy on our current picture of star formation in low mass galaxies is considered.KeywordsStar FormationFlux RatioDwarf GalaxyStar Formation RateInitial Mass FunctionThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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