Reionisation, chemical enrichment and seed black holes from the first stars: is Population III important?

Details Reionisation, chemical enrichment and seed black holes from the first stars: is Population III important? Reionisation, chemical enrichment and seed black holes from the first stars: is Population III important?

2003-10-13

arxiv.org/abs/astro-ph/0310331v3

Mon.Not.Roy.Astron.Soc.350:539,2004

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS. 13 pages, including 9 figures and 2 tables

Scientific paper

10.1111/j.1365-2966.2004.07662.x

We investigate the effects of a top-heavy stellar initial mass function on the reionisation history of the intergalactic medium (IGM). We use cosmological simulations that include self-consistently the feedback from ionising radiation, H_2 dissociating radiation and supernova (SN) explosions. We find that it is difficult to reionise the IGM at z_rei>10 with stellar sources even after making extreme assumptions. If star formation in 10^9 M_\odot galaxies is not suppressed by SN explosions, the optical depth to Thomson scattering is tau_e< 0.13. If we allow for the normal energy input from SNe or if pair-instability SNe are dominant, we find taue<0.09. Assuming normal yields for the first stars (popIII), the mean metallicity of the IGM is already Z/Z_\odot=2x10^-3 (10^-3260 M_\odot, they collapse directly onto black holes without exploding as SNe.If metal-poor stars are initially important and collapse to black holes is the typical outcome, then the secondary emission of ionising radiation from accretion on SN induced seed black holes, might be more important than the primary emission. Surprisingly, including feedback effects, we estimate that a warm dark matter scenario (with particle mass of 1.25 keV) reduces tau_e by only approximately 10%.[abridged]

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