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Cosmic Evolution of Gas Content and Accretion

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Lessons from the Local Group

Abstract

In the present universe, the gas is a minor component of giant galaxies, and its dominant phase is atomic (HI). During galaxy evolution in cosmic times, models predict that gas fractions were much higher in galaxies, and gas phases could be more balanced between molecular (H2) and atomic (HI). This gaseous evolution is certainly a key factor to explain the cosmic evolution of the star formation rate density. Star formation efficiency might also vary with redshift, and the relative importance of these factors is not yet well known. Our current knowledge of cosmic evolution of gas from molecular observations at high-z is reviewed and confronted with simulations.

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Acknowledgements

My great thanks to the organisers of this wonderful meeting with wide scientific interests. The European Research Council is gratefully acknowledged for the Advanced Grant Program Num 267399-Momentum.

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Authors and Affiliations

  1. Observatoire de Paris, LERMA, CNRS, 61 Av. de l’Observatoire, 75014, Paris, France

    Françoise Combes

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  1. Françoise Combes
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Correspondence to Françoise Combes .

Editor information

Editors and Affiliations

  1. Australian National University, Canberra, Australia

    Kenneth Freeman

  2. IBM T.J. Watson Research Center, Yorktown Heights, New York, USA

    Bruce Elmegreen

  3. University of the Witwatersrand, Johannesburg, South Africa

    David Block

  4. University of the Witwatersrand, Johannesburg, South Africa

    Matthew Woolway

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© 2015 Springer International Publishing Switzerland

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Combes, F. (2015). Cosmic Evolution of Gas Content and Accretion. In: Freeman, K., Elmegreen, B., Block, D., Woolway, M. (eds) Lessons from the Local Group. Springer, Cham. https://doi.org/10.1007/978-3-319-10614-4_34

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