Abstract – Galaxy Reionization
The process of reionization is now believed to have proceeded in an orchestrated manner
beginning with UV photons emitted by high redshift galaxies containing a large
fraction of Population III stars carving out ionised regions around them. The physics
during this era can be studied with a combination of redshifted 21-cm spin-flip transition
tracing neutral hydrogen gas, IR emission from massive primordial stars that trace
the global star-formation rate during reionization, and the imprint of hot-electrons
in first supernovae remnants Compton-cooling off of cosmic microwave background
(CMB) radiation through the Sunyaev-Zel’dovich effect. While these individual effects
and their observable signatures have been advocated as probes of reionization
history, here we show how cross-correlation studies between these signals can be used
to further understand physics during reionization. Cross-correlation studies are advantageous
since the measurable statistics do not suffer in the same manner from
foregrounds and systematic effects as is the case of auto-correlation function measurements.
We discuss the prospects for detecting various cross-correlation statistics using
present and next generation experiments and the information related to reionization
captured by them.
Key words: cosmology: theory — large scale structure infrared:galaxy general — stars:
formation — cosmology: observations — diffuse radiation
