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UV to IR Models of Galaxy Evolution and Cosmology

Published online by Cambridge University Press:  07 August 2017

Brigitte Rocca-Volmerange
Brigitte Rocca-Volmerange*
Affiliation:
Institut d'Astrophysique 98 bis Bd Arago F-75014 PARIS

Abstract

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Recent improvements of spectrophotometric evolutionary models are described. New stellar libraries in the near-infrared (JHK) allow extension of the synthetic spectral Atlas of galaxies down to 10μm. From analyses in the far-UV and visible, observed colors and counts of faint galaxies are fitted by modelling a standard luminosity evolution and a low value of ωo(≃ 0.1) while, in a ωo=1 Universe, models only fit data with a standard luminosity evolution and a number density evolution ≃ (1 + z)1.8: such a modelling is simulating a merging process. Another solution would be a tidally triggered star formation rate in a model in which galaxies form by hierarchical clustering of a dominant dark matter component. From evolution of M/L ratio, these models allow to link observed luminosity functions with mass distributions predicted from galaxy formation models and then to significantly connect evolution to formation models. Nevertheless these two models are not sufficient to fit some observational data such as the Hubble diagrams and faint galaxy counts in the near-infrared, the bright galaxy counts in visible and the Extragalactic Background Light. So new evolution scenarios are needed implying other constraints for cosmological parameters.

Type
III. The Stellar Populations of Non-Resolved Galaxies
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 357 - 366
Copyright
Copyright © Kluwer 

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