The Evolution of the Star and Gas Content of Galaxies
22-Oct-99
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Table of Contents
Title
Why stars and gas?
Basic galaxy formation models
A global view of the low-z universe
Dust opacity in the local universe
Cosmic background light
Is the present the peak of opacity?
Metals and dust vs redshift
Is the young universe metal-poor?
Data on DLAs
Dust obscuration at high-z - I
Effect of dust distribution inside galaxies - I
Effect of dust distribution inside galaxies - II
Dust obscuration at high-z - II
Spectral tests
UV continuum slope versus redshift
UV-select sample of local starbursts
No assumptions as to dust geometry
Reddening/extinction versus wavelength
Dust at z=3
The other test for dust at high-z
Relation between SCUBA and Ly-break galaxies?
NGC6090
ISO observations and FIR fluxes
NGC6090 / NGC7673 / TOL1924-416
What determines similarities and differences?
Predicted FIR flux densities at z=1
Predicted FIR flux densities at z=3
Will Ly-break galaxies be detected with SCUBA?
Challenge: a model satisfying all constraints
Observational constraints
History of the observed UV light
Cosmic IR background
Galaxy model
Models: SFR versus redshift
Model 3 - history
Model 3 - extinction
Model 2 - extinction
Model 3 - cosmic IR background
Model 2 - cosmic IR background
Model 3 - T and F
FIR
Model 2 - T and F
FIR
Comparisons of models and observations
Conclusions - I
Conclusions - II
Author:
Daniela Calzetti
Email:
calzetti@stsci.edu
