Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-24T06:43:45.650Z Has data issue: false hasContentIssue false
  • English
  • Français

Using Negative Detections to Estimate Source-Finder Reliability

Published online by Cambridge University Press:  02 January 2013

P. Serra ,
R. Jurek  and
L. Flöer
P. Serra*
Affiliation:
Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands
R. Jurek
Affiliation:
CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia
L. Flöer
Affiliation:
Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany
*
DCorresponding author. Email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We describe a simple method to determine the reliability of source finders based on the detection of sources with both positive and negative total flux. Under the assumption that the noise is symmetric and that real sources have positive total flux, negative detections can be used to assign to each positive detection a probability of being real. We discuss this method in the context of upcoming, interferometric Hi surveys.

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. 296 - 300
Copyright
Copyright © Astronomical Society of Australia 2012

References

Dickinson, M., et al. , 2004, ApJL, 600, L99CrossRefGoogle Scholar
Irwin, J. O., 1937, J. R. Stat. Soc., 100, 415CrossRefGoogle Scholar
Jurek, R., 2011, ArXiv 1112.1561Google Scholar
Kim, M., et al. , 2007, ApJS, 169, 401CrossRefGoogle Scholar
Koribalski, B. S. & Staveley-Smith, L., 2009, ASKAP Survey Science Proposal, available at http://www.atnf.csiro.au/research/WALLABYGoogle Scholar
Kovač, K., Oosterloo, T. A. & van der Hulst, J. M., 2009, MNRAS, 400, 743CrossRefGoogle Scholar
Meyer, M. J., et al. , 2004, MNRAS, 350, 1195CrossRefGoogle Scholar
Popping, A., Westmeier, T., Jurek, R., Serra, P., Flöer, L., Meyer, M. J. & Koribalski, B. S., 2012, PASA Special Issue on Source Finding and Visualization, ArXiv 1201.3994Google Scholar
Saintonge, A., 2007, AJ, 133, 2087CrossRefGoogle Scholar
Serra, P., et al. , 2011, ArXiv 1111.4241Google Scholar
van der Hulst, J. M., 2002, ASPC, 276, 84Google Scholar
Verheijen, M., Oosterloo, T., Heald, G. & van Cappellen, W., 2009, in Proceedings of Panoramic Radio Astronomy: Wide-Field 1–2 GHz Research on Galaxy Evolution, ed. Heald, G. & Serra, P. (Groningen, The Netherlands: Proceedings of Science), PoS(PRA2009)010Google Scholar
Westmeier, T., Popping, A. & Serra, P., 2012, PASA, Special Issue on Source Finding and VisualizationGoogle Scholar
Yan, H. & Windhorst, R. A., 2004, ApJL, 612, L93CrossRefGoogle Scholar
Zwaan, M. A., et al. , 2004, MNRAS, 350, 1210CrossRefGoogle Scholar