The Importance of HI to the Gastrophysics of Galaxies

Details The Importance of HI to the Gastrophysics of Galaxies The Importance of HI to the Gastrophysics of Galaxies

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21511401h&link_type=abstract

American Astronomical Society, AAS Meeting #215, #114.01; Bulletin of the American Astronomical Society, Vol. 42, p.563

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In contrast to the wealth of detail available for the stellar component, quantitative measures of the gas content of galaxies are limited to only a few tens of thousands of objects, and of the gas distribution within them, to only hundreds. And, although cold gas contributes only a piffling amount of the total baryon content of the universe, the atomic hydrogen 21 cm (HI) line has played a pivotal role in our understanding of galaxies and their evolution. Because of its simple physics and value as a kinematic tracer, the HI line emission profile yields a robust measure of the neutral gas mass, measuring the gas content within and around galaxies, tracing the dark matter potential and probing volumes and objects that other survey tracers may not. Particularly from the perspective of the Arecibo Legacy Fast ALFA (ALFALFA) survey and the associated multiwavelength studies that have sprouted from it, this review will remind us how many gas rich galaxies there really are, where those reside and how the local HI census provides fundamental insight into how galaxies accrete gas, form stars and interact with their environment.
The commitment, efforts and enthusiasm of the ALFALFA team and support from NSF grant AST-0607007 and the Brinson Foundation are gratefully acknowledged.

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