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Chemical Constraints, Baryonic Mass and the Chemical Evolution of Low Surface Brightness Galaxies

Published online by Cambridge University Press:  12 April 2016

M.G. Edmunds
M.G. Edmunds*
Affiliation:
Department of Physics and Astronomy, Cardiff University, P.O. Box 913, Cardiff, CF2 3YB, U.K.

Abstract

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A brief review of primordial helium and deuterium abundances suggests a baryonic mass density of ΩB ≈ 0.04 – 0.045 (for Ho = 70). This mass may be dominated by intergalactic gas in clusters and groups of galaxies. The observed low chemical abundances in evolved dwarf galaxies might suggest that outflow was the origin for such gas, and we make general suggestions for the interpretation of the data from the next generation of X-ray spectroscopic satellites. The effects of both outflow and inflow on the chemical evolution of galaxies is discussed, particularly in the context of low surface brightness galaxies, and we comment on their dust content.

Type
The baryonic mass content of the Universe
Information
International Astronomical Union Colloquium , Volume 171: The Low Surface Brightness Universe , 1999 , pp. 383 - 389
Copyright
Copyright © Astronomical Society of the Pacific 1999

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