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Title:
The ASKAP/EMU Source Finding Data Challenge
Authors:
Hopkins, A. M.; Whiting, M. T.; Seymour, N.; Chow, K. E.; Norris, R. P.; Bonavera, L.; Breton, R.; Carbone, D.; Ferrari, C.; Franzen, T. M. O.; Garsden, H.; González-Nuevo, J.; Hales, C. A.; Hancock, P. J.; Heald, G.; Herranz, D.; Huynh, M.; Jurek, R. J.; López-Caniego, M.; Massardi, M.; Mohan, N.; Molinari, S.; Orrù, E.; Paladino, R.; Pestalozzi, M.; Pizzo, R.; Rafferty, D.; Röttgering, H. J. A.; Rudnick, L.; Schisano, E.; Shulevski, A.; Swinbank, J.; Taylor, R.; van der Horst, A. J.
Affiliation:
AA(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), AB(CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia), AC(International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia), AD(CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia), AE(CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia), AF(Instituto de Física de Cantabria (CSIC-UC), Santander, 39005 Spain), AG(Jodrell Bank Centre for Astrophysics, The University of Manchester, Manchester, M13 9PL, UK), AH(Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, the Netherlands), AI(Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Blvd de l'Observatoire, CS 34229, 06304 Nice cedex 4, France), AJ(International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia), AK(Laboratoire AIM (UMR 7158), CEA/DSM-CNRS-Université Paris Diderot, IRFU, SEDI-SAP, Service dAstrophysique, Centre de Saclay, F-91191 Gif-Sur-Yvette cedex, France), AL(Departamento de Física, Universidad de Oviedo, C. Calvo Sotelo s/n, 33007 Oviedo, Spain; Instituto de Física de Cantabria (CSIC-UC), Santander, 39005 Spain), AM(National Radio Astronomical Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801-0387, USA; Jansky Fellow, National Radio Astronomical Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801-0387, USA), AN(International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia; Sydney Institute for Astronomy, School of Physics A29, The University of Sydney, NSW 2006, Australia; ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), The University of Sydney, NSW 2006, Australia), AO(ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, the Netherlands; University of Groningen, Kapteyn Astronomical Institute, Landleven 12, 9747 AD Groningen, the Netherlands), AP(Instituto de Física de Cantabria (CSIC-UC), Santander, 39005 Spain), AQ(International Centre for Radio Astronomy Research, M468, University of Western Australia, Crawley, WA 6009, Australia), AR(CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia), AS(European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain; Instituto de Física de Cantabria (CSIC-UC), Santander, 39005 Spain), AT(INAF-Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy), AU(National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Post Bag 3, Ganeshkhind, Pune 411 007, India), AV(IAPS - INAF, via del Fosso del Cavaliere 100, I-00173 Roma, Italy), AW(ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, the Netherlands), AX(Department of Physics and Astronomy, University of Bologna, V.le Berti Pichat 6/2, 40127 Bologna, Italy; INAF-Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy), AY(IAPS - INAF, via del Fosso del Cavaliere 100, I-00173 Roma, Italy), AZ(ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, the Netherlands), BA(Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany), BB(Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA, the Netherlands), BC(Minnesota Institute for Astrophysics, University of Minnesota, 116 Church St. SE, Minneapolis, MN 55455), BD(IAPS - INAF, via del Fosso del Cavaliere 100, I-00173 Roma, Italy), BE(ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, the Netherlands; University of Groningen, Kapteyn Astronomical Institute, Landleven 12, 9747 AD Groningen, the Netherlands), BF(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, the Netherlands), BG(Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch, 7701, South Africa; Department of Physics, University of the Western Cape, Robert Sobukwe Road, Bellville, 7535, South Africa), BH(Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052, USA; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, the Netherlands)
Publication:
Publications of the Astronomical Society of Australia, Volume 32, id.e037 23 pp. (PASA Homepage)
Publication Date:
10/2015
Origin:
CUP
Astronomy Keywords:
methods: data analysis, radio continuum: general, techniques: image processing
Abstract Copyright:
2015: Astronomical Society of Australia
DOI:
10.1017/pasa.2015.37
Bibliographic Code:
2015PASA...32...37H

Abstract

The Evolutionary Map of the Universe (EMU) is a proposed radio continuum survey of the Southern Hemisphere up to declination + 30°, with the Australian Square Kilometre Array Pathfinder (ASKAP). EMU will use an automated source identification and measurement approach that is demonstrably optimal, to maximise the reliability and robustness of the resulting radio source catalogues. As a step toward this goal we conducted a "Data Challenge" to test a variety of source finders on simulated images. The aim is to quantify the accuracy and limitations of existing automated source finding and measurement approaches. The Challenge initiators also tested the current ASKAPsoft source-finding tool to establish how it could benefit from incorporating successful features of the other tools. As expected, most finders show completeness around 100% at ≈ 10sigma dropping to about 10% by ≈ 5sigma. Reliability is typically close to 100% at ≈ 10sigma, with performance to lower sensitivities varying between finders. All finders show the expected trade-off, where a high completeness at low signal-to-noise gives a corresponding reduction in reliability, and vice versa. We conclude with a series of recommendations for improving the performance of the ASKAPsoft source-finding tool.
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