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The Structure of Halo Gas around M33

Published online by Cambridge University Press:  21 March 2017

Olivia C. Keenan ,
Jonathan I. Davies ,
Rhys Taylor  and
Robert F. Minchin
Olivia C. Keenan
Affiliation:
School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, U.K. email: olivia.keenan@astro.cf.ac.uk
Jonathan I. Davies
Affiliation:
School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, U.K. email: olivia.keenan@astro.cf.ac.uk
Rhys Taylor
Affiliation:
Astronomical Institute of the ASCR, Boční II 1401, 14100, Prague, Czech Republic
Robert F. Minchin
Affiliation:
Arecibo Observatory, HC03 Box 53995, Arecibo, Puerto Rico 00612
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Abstract

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Understanding the distribution of gas in and around galaxies is vital for our interpretation of galaxy formation and evolution. As part of the Arecibo Galaxy Environment Survey (AGES) we have observed the neutral hydrogen (HI) gas in and around the nearby Local Group galaxy M33 to a greater depth than previous observations. As part of this project we investigated the absence of optically detected dwarf galaxies in its neighbourhood, which is contrary to predictions of galaxy formation models. We observed 22 discrete clouds, 11 of which were previously undetected and none of which have optically detected counterparts. We find one particularly interesting hydrogen cloud, which has many similar characteristics to hydrogen distributed in the disk of a galaxy. This cloud, if it is at the distance of M33, has a HI mass of around 107 M⊙ and a diameter of 18 kpc, making it larger in size than M33 itself.

Keywords

galaxies: clusters: generalgalaxies: dwarf(galaxies:) Local Groupradio lines: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 244 - 247
Copyright
Copyright © International Astronomical Union 2017 

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