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Baryonic Dark Matter and the Chemical Evolution of Galaxies

  • Chapter
Baryonic Dark Matter

Part of the book series: NATO ASI Series ((ASIC,volume 306))

Abstract

Reasonable inhomogeneous Big Bang nucleosynthesis models suggest (in usual notation). 009 ≤ Ω B h 20 ≤ .04 corresponding to typical mass:light ratios between 13 h-1 and 60 h-1 if there is no large undetected luminosity density due to obscured or low surface brightness galaxies. The lower limits are large in relation to what is seen in the solar neighbourhood, which latter is quite in accordance with a reasonable model of galactic chemical evolution. Larger mass:light ratios occur (and are expected) in elliptical galaxies, but these make only a minor contribution to the overall average.

The conclusion is that baryonic dark matter exists either in some form that is radiatively and nuclearly inactive (eg ‘Jupiters’) and separate spatially from visible stellar populations — eg in galactic dark halos — or in the form of galaxies that are still undetected (or whose luminosity has been underestimated) in optical surveys owing to low surface brightness and/or obscuration. Chemical evolution considerations offer only a few negative clues as to its nature and distribution.

“Oh dear, what can the matter be?” (Traditional English song)

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  1. B. E. J. Pagel

    Present address: NORDITA, Blegdamsvej 17, DK-2100, Copenhagen 0, Denmark

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  1. Royal Greenwich Observatory, Herstmonceux Castle, Hailsham, E Sussex, BN27 1RP, UK

    B. E. J. Pagel

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  1. Institute of Astronomy & Clare College, Madingley Road, Cambridge, UK

    D. Lynden-Bell

  2. Institute of Astronomy & King’s College, Madingley Road, Cambridge, UK

    G. Gilmore

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Pagel, B.E.J. (1990). Baryonic Dark Matter and the Chemical Evolution of Galaxies. In: Lynden-Bell, D., Gilmore, G. (eds) Baryonic Dark Matter. NATO ASI Series, vol 306. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0565-8_14

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