  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.
