Radiative Transfer Simulations of Cosmic Reionization With Pop II and III Stars

Details Radiative Transfer Simulations of Cosmic Reionization With Pop II and III Stars Radiative Transfer Simulations of Cosmic Reionization With Pop II and III Stars

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990..445t&link_type=abstract

FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 445-449 (2008).

Computer Science

Cosmology, Radiative Transfer, Scattering, Intergalactic Matter, Quasar Absorption And Emission-Line Systems, Lyman Forest, Star Formation, Population Ii Stars, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies

Scientific paper

We have simulated 3 large volume, high resolution realizations of cosmic reionization using a hybrid code that combines a N-body algorithm for dark matter, prescriptions for baryons and star formation, and a radiative transfer algorithm for ionizing photons. Our largest simulation, with 24 billion particles in a 100 Mpc/h box, simultaneously provides (1) the mass resolution needed to resolve dark matter halos down to a virial temperatures of 104 K and (2) the volume needed to fairly sample highly biased sources and large HII regions. We model the stellar initial mass function (IMF) by following the spatially dependent gas metallicity evolution, and distinguish between the first generation (Population III) stars and the second generation (Population II) stars. The Population III stars, with a top-heavy IMF, produce an order of magnitude more ionizing photons at high redshifts z>~10, resulting in a more extended reionization. In our simulations, complete overlap of HII regions occurs at z~6.5 and the computed mass and volume weighted residual HI fractions at 5<~z<~6.5 are both in good agreement with high redshift quasar absorption measurements from SDSS. The values for the Thomson optical depth are consistent within 1-σ of the current best-fit value from the WMAP Year 3 data release.

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