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Article Contents
- ABSTRACT
- 8.1.STAR-FORMING MOLECULAR CLOUDS
- 8.1.1.Background
- 8.1.2.Molecular excitation
- 8.1.2.1.Summary
- 8.1.3.Observed properties
of molecular gas
- 8.1.3.1.Self-gravitating
GMCs
- 8.1.3.2.Molecular masses
from
≫ 1 CO
emission
- 8.1.3.3.Lifetimes of
GMCs
- 8.1.3.4.GMC supersonic
internal motions
- 8.1.3.5.Summary
- 8.2.STAR FORMATION
- 8.2.1.Probes of star
formation
- 8.2.2.Infrared emission
- 8.2.3.Dust optical depth:
< 1 or
> 1?
- 8.2.4.Dust temperature of the
emergent luminosity
- 8.2.5.Star formation rate
from LIR
- 8.2.6.Dust and ISM mass
estimates
- 8.2.7.Effective source size
- 8.2.8.Luminosity and SFR
estimates from submm continuum
- 8.2.9.Modelling
optically-thick dust clouds
- 8.2.10.Summary
- 8.3.STAR FORMATION IN GALAXIES -
TWO MODES
- 8.3.1.Quiescent or normal
mode of star formation
- 8.3.2.Dynamically-driven
starburst mode
- 8.3.3.Star formation `laws'
- 8.3.4.Distinguishing normal
star formation and starbursts: concentration and timescales
- 8.3.5.Starbursts in ULIRGs
- 8.3.6.Arp 220 - a
prototypical ULIRG
- 8.3.7.An aside: Sgr A* - an
extraordinary ISM
- 8.3.8.Nuclear starburst
disks
- 8.3.9.Maximum-rate
starbursts - the dust Eddington limit
- 8.3.10.AGN - starburst:
observational connections
- 8.3.11.AGN - starburst:
theoretical connections
- 8.4.EVOLUTION OF GALAXIES AT HIGH
REDSHIFT
- 8.4.1.Luminosity and Mass
Functions
- 8.4.2.Environmental
correlations
- 8.5.MODELLING STAR FORMATION AT HIGH
REDSHIFT: SAME MODES BUT DIFFERENT FREQUENCY
- 8.5.1.Cosmic evolution:
M* and MISM and star formation
luminosities
- 8.5.2.Need ISM
replenishment by accretion
- 8.5.3.ULIRG starbursts
account for high-L tail
- 8.6.CONCLUSIONS
- REFERENCES