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HI in the outskirts of Nearby Spirals

Published online by Cambridge University Press:  21 March 2017

Elias Brinks  and
António Portas
Elias Brinks
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, United Kingdom email: [email protected]
António Portas
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, United Kingdom email: [email protected] Marketing Department, Leeds Beckett University, Leeds LS1 3HE, United Kingdom email: [email protected]
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Abstract

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We analyse nine galaxies taken from the THINGS survey to investigate the H I extent of spiral galaxy disks. We exploit the high spatial and velocity resolution, and the sensitivity of THINGS to investigate where the atomic gas disks end and what might shape their outskirts. We find that the atomic gas surface density across most of the disk is constant at 5 to 10 M⊙ pc−2 and declines at large radius. The shape of the H I distribution can be described by a Sérsic–type function with a slope index n = 0.18 – 0.36. The H I column density at which radial profiles turn over is found to be at too high a level for it to be caused by ionisation by a meta–galactic UV field. Instead we suggest the H I extent is rather set by how galaxy disks form.

Keywords

galaxies: structuregalaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 235 - 237
Copyright
Copyright © International Astronomical Union 2017 

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