A Model of Metallicity Evolution in the Early Universe

Abstract

We apply the phenomenological model used to explain the abundances of Fe and r-process elements in very metal-poor stars in the Galaxy to [Fe/H] of damped Ly alpha systems. It is assumed that the first stars formed after the Big Bang were very massive and promptly enriched the interstellar medium to [Fe/H] ~ -3, at which metallicity formation of normal stars took over. Subsequent Fe enrichment was provided by Type II supernovae. The range of [Fe/H] at a given redshift z for damped Ly alpha systems is explained by the time t* after the Big Bang at which normal star formation started in an individual protogalactic system. The average t* is approx 80% the age of the universe for damped Ly alpha systems at z approx 1.5 to 4.5, indicating a long delay between the Big Bang and the turn-on of protogalaxies. It is inferred that a substantial fraction of the total baryonic matter may not have been aggregated into protogalaxies where normal star formation had occurred down to z ~ 1.5. The data near z = 2.2 suggest that the rate of turn-on of protogalaxies was initially very low and slowly reached a maximum at ~ 3 Gyr after the Big Bang. This may be important in understanding the rate of formation of quasars.

13 pages, 4 figures, to appear in ApJ Letters

References in corpus (6)

• Forming the First Stars in the Universe: The Fragmentation of Primordial Gas
• Intervening O VI Quasar Absorption Systems at Low Redshift: A Significant Baryon Reservoir
• Evidence of Multiple r-Process Sites in the Early Galaxy: New Observations of CS 22892-052
• Metallicity Evolution in the Early Universe
• Prompt Iron Enrichment, Two r-Process Components, and Abundances in Very Metal-Poor Stars
• Stellar Abundances in the Early Galaxy and Two r-Process Components

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• Galactic Chemical Abundances at z>3 I: First Results from the Echellette Spectrograph and Imager
• The Implications of the New Z=0 Stellar Models and Yields on the Early Metal Pollution of the Intergalactic Medium
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