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Constraints on the molecular gas content of galaxies at high redshift arecrucial to further our understanding of star formation and galaxy evolutionthrough cosmic times, as molecular gas is the fuel for star formation. Sinceits initial detection at large cosmic distances almost two decades ago, studiesof molecular gas in the early universe have come a long way. We have detectedCO emission from >100 galaxies, covering a range of galaxy populations at z>1,reaching out to z>6, down to sub-kpc scale resolution, and spanning ~2 ordersof magnitude in gas mass (aided by gravitational lensing). Recently, it haseven become possible to directly identify distant galaxies through theirmolecular emission lines without prior knowledge of their redshifts. The newgeneration of powerful long wavelength interferometers such as the ExpandedVery Large Array (EVLA) and Atacama Large (sub)Millimeter Array (ALMA) thushold the promise to liberate studies of molecular gas in high redshift galaxiesfrom their heavy pre-selection. This will enable more systematic studies of themolecular gas content in star-forming galaxies back to the earliest cosmictimes.

Constraints on the Star-Forming Interstellar Medium in Galaxies Back to the First Billion Years of Cosmic Time