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Scientific Background to the UKST Hα Survey

Published online by Cambridge University Press:  05 March 2013

M. R. W. Masheder ,
S. Phillipps  and
Q. A. Parker
M. R. W. Masheder
Affiliation:
Astrophysics Group, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK; Mike.Masheder@bristol.ac.uk
S. Phillipps
Affiliation:
Astrophysics Group, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK; S.Phillipps@bristol.ac.uk
Q. A. Parker
Affiliation:
Anglo-Australian Observatory, Siding Spring, Coonabarabran, NSW 2357, Australia; qap@aaocbnu1.aao.gov.au
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Abstract

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The dominant process in the evolution of spiral galaxies like our own is clearly the formation of new stars, and the leading optical indicator of this is Hα emission. Considering the tremendous importance of star formation and its variation within and between galaxies, it is surprising just how little survey work has been carried out at Hα. After the successful development of Tech Pan films for deep photographic imaging with the UKST, and given the particular sensitivity of Tech Pan at wavelengths near Hα, it was natural to consider the possibilities for a narrowband Hα imaging survey of large angular extent. This idea quickly developed into a full-blown survey of the whole of the Southern Milky Way, of the Magellanic Clouds, and of selected extragalactic regions of interest such as that around the Virgo Cluster. This special issue is devoted to the discussion of the details of making and using this survey.

Keywords

surveysstars: formationISM: atomsHII regionsgalaxies: general
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 15 , Issue 1 , 1998 , pp. 5 - 8
Copyright
Copyright © Astronomical Society of Australia 1998

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