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Article Contents

ABSTRACT

1.INTRODUCTION
1.1.Motivation
1.2.Galaxy formation and the need for cool gas observations

2.CONCEPTS OF OBSERVING COOL GAS
2.1.Heating and cooling of the starforming ISM in galaxies
2.2.Tracing molecular gas: observable frequencies
2.3.Gas Temperatures & Critical Density
2.4.Brightness Temperature and line luminosities
2.5.CO luminosity to total molecular gas mass conversion factor
2.6.Modeling the line excitation
2.7.Water lines
2.8.Atomic Fine Structure lines
2.9.Relation to far-infrared emission and SFRs
2.10.Role of CMB

3.MOLECULAR GAS AT HIGH REDSHIFT
3.1.Introduction
3.2.Quasars
3.3.Submillimeter galaxies
3.4.Radio Galaxies
3.5.Color Selected Star-Forming Galaxies (CSG)
3.6.MIPS/24 micron-selected Galaxies
3.7.Lyman–Break Galaxies, Lyα Emitters, and Lyα Blobs
3.8.Table of all high-z ISM detections
3.9.Historical note

4.OBSERVATIONAL DIAGNOSIS OF THE COOL ISM IN DISTANT GALAXIES
4.1.Molecular gas excitation
4.2.CO luminosity to total molecular gas mass conversion
4.3.Atomic Fine Structure lines
4.4.Dense gas tracers and other molecules at high redshift
4.5.Star formation laws and gas consumption
4.6.Imaging of the molecular gas in early galaxies
4.7.Outflows

5.DENSE GAS HISTORY OF THE UNIVERSE
5.1.Gas dominated disks during the epoch of galaxy assembly
5.2.First Galaxies
5.3.Spectral Deep Fields and the Dense Gas History of the Universe

6.SUMMARY POINTS / CONCLUDING REMARKS

7.FUTURE DIRECTIONS

REFERENCES