Cosmological galaxy formation

A. H. Nelson (Cardiff) (The Virgo Consortium); A. Jenkins (Durham); C. S. Frenk (Durham); F. R. Pearce (Durham); G. Efstathiou (Cambridge); H. M. P. Couchman (UWO); J. A. Peacock (Edinburgh); J. M. Colberg (MPA); P. A. Thomas (Sussex); S. D. M. White (MPA)

arxiv: astro-ph/9906032 · v1 · submitted 1999-06-02 · 🌌 astro-ph

Cosmological galaxy formation

F. R. Pearce (Durham) , C. S. Frenk (Durham) , A. Jenkins (Durham) , J. M. Colberg (MPA) , P. A. Thomas (Sussex) , H. M. P. Couchman (UWO) , S. D. M. White (MPA) , G. Efstathiou (Cambridge)

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J. A. Peacock (Edinburgh) A. H. Nelson (Cardiff) (The Virgo Consortium)

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keywords galaxycorrelationcosmologicalformationobservedalmostamplitudeback

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We discuss the first results from two successful simulations of galaxy formation within a cosmological volume. With over 2000 large objects forming in each we have sufficient numbers to reliably produce both galaxy correlation and luminosity functions. We find that the observed galaxy counts are well fitted by these models and that the galaxies display an almost un-evolving correlation function back to a redshift of 3 which closely resembles the featureless observed form and amplitude.

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Cosmological galaxy formation

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