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The Gas Phase in a Low Metallicity ISM

Published online by Cambridge University Press:  01 June 2008

Elias Brinks ,
Se–Heon Oh ,
Ioannis Bagetakos ,
Frank Bigiel ,
Adam Leroy ,
Antonio Usero ,
Fabian Walter ,
W. J. G. de Blok  and
Robert C. Kennicutt Jr.
Elias Brinks
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
Se–Heon Oh
Affiliation:
Research School of Astronomy & Astrophysics, The Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia
Ioannis Bagetakos
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
Frank Bigiel
Affiliation:
Max–Plank–Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany
Adam Leroy
Affiliation:
Max–Plank–Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany
Antonio Usero
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
Fabian Walter
Affiliation:
Max–Plank–Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany
W. J. G. de Blok
Affiliation:
Univ. of Cape Town, Dept. of Astronomy, Private Bag X3, Rondebosch 7701, South Africa
Robert C. Kennicutt Jr.
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
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Abstract

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We present several results from our analysis of dwarf irregular galaxies culled from The HI Nearby Galaxy Survey (THINGS). We analyse the rotation curves of two galaxies based on “bulk” velocity fields, i.e. velocity maps from which random non–circular motions are removed. We confirm that their dark matter distribution is best fit by an isothermal halo model. We show that the star formation properties of dIrr galaxies resemble those of the outer parts of larger, spiral systems. Lastly, we study the large scale (3–D) distribution of the gas, and argue that the gas disk in dIrrs is thick, both in a relative, as well as in an absolute sense as compared to spirals. Massive star formation through subsequent supernova explosions is able to redistribute the bulk of the ISM, creating large cavities. These cavities are often larger, and longer–lived than in spiral galaxies.

Keywords

galaxies: structuregalaxies: spiralgalaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 265 - 273
Copyright
Copyright © International Astronomical Union 2008

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