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H I Imaging Surveys: Gas and Galaxy Evolution in Different Environments

Published online by Cambridge University Press:  05 December 2011

Jacqueline van Gorkom
Jacqueline van Gorkom*
Affiliation:
Department of Astronomy, Columbia University, New York, NY 10027, USA email: jvangork@astro.columbia.edu
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Abstract

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Our understanding of the formation and evolution of galaxies and the large scale structure has advanced enormously over the last decade, thanks to an impressive synergy between theoretical and observational efforts. While the growth of the dark matter component seems well understood, the physics of the gas, during its accretion, removal and/or depletion is less well understood. Increasingly large scale optical surveys are tracing out the cosmic web of filaments and voids and mathematical tools have been developed to describe these structures and identify galaxies in specific environments. H I imaging surveys begin to answer the question: how do galaxies get and lose their gas. The best evidence for ongoing gas accretion is found in the lowest density environments, while removal of gas in the highest density environments stops star formation and reddens the galaxies. Although current H I emission surveys are limited to redshifts less than 0.2, this is where the LSS is best defined and much can be learned in the local universe.

Keywords

galaxiesevolutionISMlarge-scale structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 41 - 46
Copyright
Copyright © International Astronomical Union 2011

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