4 research outputs found
Simulating Cosmic Reionization at Large Scales I: the Geometry of Reionization
We present the first large-scale radiative transfer simulations of cosmic
reionization, in a simulation volume of (100/h Mpc)^3, while at the same time
capturing the dwarf galaxies which are primarily responsible for reionization.
We achieve this by combining the results from extremely large, cosmological,
N-body simulations with a new, fast and efficient code for 3D radiative
transfer, C^2-Ray. The resulting electron-scattering optical depth is in good
agreement with the first-year WMAP polarization data. We show that reionization
clearly proceeded in an inside-out fashion, with the high-density regions being
ionized earlier, on average, than the voids. Ionization histories of
smaller-size (5 to 10 comoving Mpc) subregions exibit a large scatter about the
mean and do not describe the global reionization history well. The minimum
reliable volume size for such predictions is ~30 Mpc. We derive the
power-spectra of the neutral, ionized and total gas density fields and show
that there is a significant boost of the density fluctuations in both the
neutral and the ionized components relative to the total at arcminute and
larger scales. We find two populations of HII regions according to their size,
numerous, mid-sized (~10 Mpc) regions and a few, rare, very large regions tens
of Mpc in size. We derive the statistical distributions of the ionized fraction
and ionized gas density at various scales and for the first time show that both
distributions are clearly non-Gaussian. (abridged)Comment: Comments: 17 pages, 17 figures, replaced to match the published
version in MNRAS. Movies and higher resolution figures can be found at
http://www.cita.utoronto.ca/~iliev/research.htm
Is a Classical Language Adequate in Assessing the Detectability of the Redshifted 21cm Signal from the Early Universe?
The classical radiometer equation is commonly used to calculate the
detectability of the 21cm emission by diffuse cosmic hydrogen at high
redshifts. However, the classical description is only valid in the regime where
the occupation number of the photons in phase space is much larger than unity
and they collectively behave as a classical electromagnetic field. At redshifts
z<20, the spin temperature of the intergalactic gas is dictated by the
radiation from galaxies and the brightness temperature of the emitting gas is
in the range of mK, independently from the existence of the cosmic microwave
background. In regions where the observed brightness temperature of the 21cm
signal is smaller than the observed photon energy, of 68/(1+z) mK, the
occupation number of the signal photons is smaller than unity. Neverethless,
the radiometer equation can still be used in this regime because the weak
signal is accompanied by a flood of foreground photons with a high occupation
number (involving the synchrotron Galactic emission and the cosmic microwave
background). As the signal photons are not individually distinguishable, the
combined signal+foreground population of photons has a high occupation number,
thus justifying the use of the radiometer equation.Comment: 4 pages, Accepted for publication in JCA