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GASKAP: The Galactic ASKAP Survey

Published online by Cambridge University Press:  21 October 2010

Snežana Stanimirovič ,
John M. Dickey ,
Steven J. Gibson ,
José F. Gómez ,
Hiroshi Imai ,
Paul A. Jones  and
Jacco Th. van Loon
Snežana Stanimirovič
Affiliation:
Dept. of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706, USA; email: [email protected]
John M. Dickey
Affiliation:
School of Maths and Physics, University of Tasmania, Private Bag 37, Hobart, TAS 7001, Australia
Steven J. Gibson
Affiliation:
Dept. of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USA
José F. Gómez
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, E-18080 Granada, Spain
Hiroshi Imai
Affiliation:
Dept. of Physics, Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065, Japan
Paul A. Jones
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia Dept. de Astronomí a, Universidad de Chile, Casilla 36-D, Santiago, Chile
Jacco Th. van Loon
Affiliation:
Astrophysics Group, Lennard Jones Laboratories, Keele University, Staffordshire, ST5 5BG, UK
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Abstract

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The Galactic Australian SKA Pathfinder (GASKAP) survey is one of several key science projects with ASKAP, a new radio telescope being built in Australia as a technology demonstrator for the Square Kilometer Array (SKA). GASKAP aims to survey about 12,779 square degrees of the Galaxy and the Magellanic System, at high spectral resolution (0.2 km s−1) and using several wavelengths: the λ21-cm HI line, the λ18-cm OH lines, and the comb of recombination lines around λ18-cm. The area covered by GASKAP includes all of the Galactic plane south of declination +40° with |b| < 10°, selected areas at higher latitudes covering important interstellar clouds in the disk and halo, the Large and Small Magellanic Clouds, and the Magellanic Bridge and Stream. Compared with previous surveys, GASKAP will achieve an order of magnitude or greater improvement in brightness sensitivity and resolution in various combinations of beam size and mapping speed matched to the astrophysical objectives.

Keywords

ISM: evolutionGalaxy: structureGalaxy: haloradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 819
Copyright
Copyright © International Astronomical Union 2010