Hα and FUV luminosities from a stochastically formed stellar population

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dc.contributor.authorNidia Danigza Lugo-López
dc.contributor.authorG. Magris
dc.contributor.authorAntonio Parravano
dc.coverage.spatialBolivia
dc.date.accessioned2026-03-22T17:27:52Z
dc.date.available2026-03-22T17:27:52Z
dc.date.issued2011
dc.description.abstractAbstract It has been observed that the ratio of Hα to FUV luminosity (L H α /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 H α /L FUV ). We present a model for the total L H α and L FUV luminosity arising from a randomly populated IMF following the Salpeter power law and the clustering law of Oey & Clarke (2007).
dc.identifier.doi10.1017/s1743921312008721
dc.identifier.urihttps://doi.org/10.1017/s1743921312008721
dc.identifier.urihttps://andeanlibrary.org/handle/123456789/64327
dc.language.isoen
dc.publisherCambridge University Press
dc.relation.ispartofProceedings of the International Astronomical Union
dc.sourceUniversidad de Los Andes
dc.subjectPhysics
dc.subjectAstrophysics
dc.subjectLuminosity
dc.subjectSurface brightness
dc.subjectInitial mass function
dc.subjectGalaxy
dc.subjectLuminosity function
dc.subjectPower law
dc.subjectStellar population
dc.subjectMass-to-light ratio
dc.titleHα and FUV luminosities from a stochastically formed stellar population
dc.typearticle

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