出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：With the three-year data, the Wilkinson Microwave Anisotropy Probe (WMAP3) produced a more
accurate determination of the electron scattering optical depth, downwarding its value fromtes =
0.17±0.08 obtained with the first-year data (WMAP1) to tes = 0.09±0.03. As a consequence,
the structure formation in the LCDM best fit model obtained WMAP3 is delayed relative to that
of WMAP1.
We show that the delay of structure formation can not fully account for the reduction of tes from
WMAP1 to WMAP3 when the radiative transfer effects and feedback mechanisms are took into
account in computing the reionization history of the Universe.
We also show that a PopIII stellar cluster with a mass of 80M⊙ and a heavy Larson initial mass
function has an ionizing efficiency high enough to account for WMAP3 results, while in the case
of WMAP1, a higher stellar mass of 1000M⊙ was required.
As the ultimate limit in constraining the reionizatin history of the Universe with PLANCK will be
placed by the our understanding of systematic effects and foregrounds removal, we discuss also
these aspects.
