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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