The evolving intergalactic medium - The uncollapsed baryon fraction in a cold dark matter universe

Details The evolving intergalactic medium - The uncollapsed baryon fraction in a cold dark matter universe The evolving intergalactic medium - The uncollapsed baryon fraction in a cold dark matter universe

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aipc..222..347s&link_type=abstract

In: After the first three minutes; Proceedings of the 1st Astrophysics Workshop, Univ. of Maryland, College Park, Oct. 15-17, 19

Astronomy and Astrophysics

Astrophysics

4

Baryons, Cosmology, Dark Matter, Galactic Evolution, Intergalactic Media, Universe, Gas Pressure, Interstellar Gas, Power Spectra, Radiative Transfer

Scientific paper

The time-varying density of the intergalactic medium (IGM) is calculated by coupling detailed numerical calculations of the thermal and ionization balance and radiative transfer in a uniform IGM of H and He to the linearized equations for the growth of density fluctuations in both gases and a dark component in a cold dark matter universe. The IGM density is identified with the collapsed baryon fraction. It is found that even if the IGM is never reheated, a significant fraction of the baryons remain uncollapsed at redshifts of four. If instead the collapsed fraction releases enough ionizing radiation or thermal energy to reionize the IGM by z greater than four as required by the Gunn-Peterson (GP) constraint, the uncollapsed fraction at z of four is even higher. The known quasar distribution is insufficient to supply the ionizing radiation necessary to satisfy the GP constraint in this case and, if stars are instead responsible, a substantial metallicity must have been produced by z of four.

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