The Formation of Dark Matter in Cooling Flows

Details The Formation of Dark Matter in Cooling Flows The Formation of Dark Matter in Cooling Flows

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.246..156t&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 246, NO. 1/SEP1, P. 156, 1990

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We propose that the unseen baryonic matter required by standard nucleosynthesis models is in the form of low-mass stars formed in cooling flows. We motivate this hypothesis by considering a hierarchical model for the formation of structure. Feedback of supernova energy limits the amount of star formation with a normal initial mass function (IMF), so that less than a half of the baryons are locked up in stars at the epoch of giant- galaxy formation. At later stages, when the ratio of the cooling time to the free-fall time of the gas in haloes exceeds unity, we suppose that the IMF becomes biased to low-mass stars, as in current-day cooling flows. Baryonic dark matter then dominates luminous matter in the largest galaxies, groups and clusters. The model explains the widespread occurrence of dark matter in these objects. It also reproduces the observed metal abundance of the intracluster medium and makes a number of other observational predictions. One of these, the copious soft X-ray emission produced by the cooling gas, can give fluxes detectable by ROSAT.

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