1932

Abstract

Over the past decade, increasingly robust estimates of the dense molecular gas content in galaxy populations between redshift = 0 and the peak of cosmic galaxy/star formation ( ∼ 1–3) have become available. This rapid progress has been possible due to the advent of powerful ground- and space-based telescopes for the combined study of several millimeter to far-IR, line or continuum tracers of the molecular gas and dust components. The main conclusions of this review are as follows:

  • ▪   Star-forming galaxies contained much more molecular gas at earlier cosmic epochs than at the present time.
  • ▪   The galaxy-integrated depletion timescale for converting the gas into stars depends primarily on or Hubble time and, at a given , on the vertical location of a galaxy along the star-formation rate versus stellar mass main sequence (MS) correlation.
  • ▪   Global rates of galaxy gas accretion primarily control the evolution of the cold molecular gas content and star-formation rates of the dominant MS galaxy population, which in turn vary with cosmological expansion. Another key driver may be global disk fragmentation in high-, gas-rich galaxies, which ties local free-fall timescales to galactic orbital times and leads to rapid radial matter transport and bulge growth. The low star-formation efficiency inside molecular clouds is plausibly set by supersonic streaming motions and internal turbulence, which in turn may be driven by conversion of gravitational energy at high and/or by local feedback from massive stars at low .
  • ▪   A simple gas regulator model is remarkably successful in predicting the combined evolution of molecular gas fractions, star-formation rates, galactic winds, and gas-phase metallicities.

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2020-08-18
2024-06-14
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