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An automatic identification of HI shells in the 2nd and 3rd Galactic Quadrants

Published online by Cambridge University Press:  01 August 2006

Soňa Ehlerová
Soňa Ehlerová*
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Bočí II 1401, 141 31 Prague, Czech Republic email: sona@ig.cas.cz
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Abstract

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We briefly discuss different methods used to identify HI shells in TB datacubes. Then we give results for our automatic method applied to LDS and LAB HI surveys of the Milky Way (2nd and 3rd quadrants). We fit the radial distribution of HI shells (the exponential profile with the scale length of 3 kpc) and the size distribution (the power law with the index of 2.1). We compare the distribution of identified HI shells with HII regions and study the differences between identifications in the 2nd and 3rd quadrants.

Keywords

ISM: bubblesmethods: data analysisGalaxy: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 91 - 95
Copyright
Copyright © International Astronomical Union 2007

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