The Dark Side of Reionization: Probing Cooling in the Early Universe

P. N. Appleton, L. Armus, A. Blain, F. Boulanger, M. Brandford, V. Bromm, C. Carilli, R-R. Chary, E. Egami, D. Frayer, M. Harwitt, G. Helou, M. Lacy, W. Latter, D. Leisawitz, C. Lonsdale, A. Ormont, P. Ogle, M. Ricotti, A. Wootten

Published 2009-03-10Version 1

Probing the growth of structure from the epoch of hydrogen recombination to the formation of the first stars and galaxies is one of the most important uncharted areas of observational cosmology. Far-IR spectroscopy covering $\lambda$ 100-500 microns from space, and narrow partial transmission atmospheric bands available from the ground, opens up the possibility of probing the molecular hydrogen and metal fine-structure lines from primordial clouds from which the first stars and galaxies formed at 6 < z $<$ 15. Building on Spitzer observations of unexpectedly powerful H2 emission from shocks, we argue that next-generation far-IR space telescopes may open a new window into the main cloud cooling processes and feedback effects which characterized this vital, but unexplored epoch. Without this window, we are essential blind to the dominant cloud cooling which inevitably led to star formation and cosmic reionization.