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Basic Testing of the duchamp Source Finder

Published online by Cambridge University Press:  02 January 2013

T. Westmeier ,
A. Popping  and
P. Serra
T. Westmeier*
Affiliation:
International Centre for Radio Astronomy Research, M468, The University of Western Australia, 35 Stirling Highway, Crawley WA 6009, Australia
A. Popping
Affiliation:
International Centre for Radio Astronomy Research, M468, The University of Western Australia, 35 Stirling Highway, Crawley WA 6009, Australia
P. Serra
Affiliation:
ASTRON, Postbus 2, 7990 AA Dwingeloo, the Netherlands
*
CCorresponding author. Email: tobias.westmeier@uwa.edu.au
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Abstract

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This paper presents and discusses the results of basic source finding tests in three dimensions (using spectroscopic data cubes) with duchamp, the standard source finder for the Australian Square Kilometre Array Pathfinder. For this purpose, we generated different sets of unresolved and extended Hi model sources. These models were then fed into duchamp, using a range of different parameters and methods provided by the software. The main aim of the tests was to study the performance of duchamp on sources with different parameters and morphologies and assess the accuracy of duchamp's source parametrisation. Overall, we find duchamp to be a powerful source finder capable of reliably detecting sources down to low signal-to-noise ratios and accurately measuring their position and velocity. In the presence of noise in the data, duchamp's measurements of basic source parameters, such as spectral line width and integrated flux, are affected by systematic errors. These errors are a consequence of the effect of noise on the specific algorithms used by duchamp for measuring source parameters in combination with the fact that the software only takes into account pixels above a given flux threshold and hence misses part of the flux. In scientific applications of duchamp these systematic errors would have to be corrected for. Alternatively, duchamp could be used as a source finder only, and source parametrisation could be done in a second step using more sophisticated parametrisation algorithms.

Keywords

methods: data analysis
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 29 , Special Issue 3: Source Finding and Visualisation , 2012 , pp. 276 - 295
Copyright
Copyright © Astronomical Society of Australia 2012

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