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Article Contents
- ABSTRACT
- 1.WHAT ARE THE DAMPED
Ly
SYSTEMS and
HOW ARE THEY FOUND?
- 1.1.History of damped
Ly Surveys
- 1.2.Modern Surveys and Identification
of damped Ly
systems
- 1.3.The Significance of the N(H I)
2 ×
1020 cm-2 Survey Threshold
2.THE NEUTRAL GAS CONTENT OF THE
UNIVERSE
2.1.Formalism
2.2.f (N, X)
2.3.d
/ dX
2.4.
g(z)
2.5.Model Comparisons
3.CHEMICAL ABUNDANCES
3.1.Methodology
3.2.Metallicity
3.3.Relative Abundances
4.IONIZED GAS
5.MOLECULAR GAS
6.KINEMATICS
7.GALAXY IDENTIFICATIONS
- 7.1.Galaxies with z
1.6
- 7.2.Galaxies with z < 1.6
- 8.STAR FORMATION IN DAMPED
Ly SYSTEMS
- 8.1.Direct Emission Measurements of
Star Formation Rates
in Damped Ly
Systems with z > 1.6
- 8.2.Star Formation Rates from the C
II* Technique
- 8.3.Implications
- 9.CHEMICAL EVOLUTION MODELS for DAMPED
Ly SYSTEMS
- 10.ARE DAMPED
Ly SAMPLES
BIASED BY DUST?
- 10.1.Observational estimates of
reddening
- 10.2.Surveys of radio-selected
QSOs
- 10.3.Empirical Estimates of Damped
Ly System
Obscuration
- 11.ARE DAMPED
Ly SAMPLES
BIASED BY GRAVITATIONAL LENSING ?
- 12.CONCLUSIONS
- REFERENCES