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Title:
A High-Resolution Foreground Model for the MWA EoR1 Field: Model and Implications for EoR Power Spectrum Analysis
Authors:
Procopio, P.; Wayth, R. B.; Line, J.; Trott, C. M.; Intema, H. T.; Mitchell, D. A.; Pindor, B.; Riding, J.; Tingay, S. J.; Bell, M. E.; Callingham, J. R.; Dwarakanath, K. S.; For, Bi-Qing; Gaensler, B. M.; Hancock, P. J.; Hindson, L.; Hurley-Walker, N.; Johnston-Hollitt, M.; Kapinska, A. D.; Lenc, E.; McKinley, B.; Morgan, J.; Offringa, A.; Staveley-Smith, L.; Wu, Chen; Zheng, Q.
Affiliation:
AA(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia; ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia), AB(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia 0000-0002-6995-4131), AC(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia; ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia), AD(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia 0000-0001-6324-1766), AE(National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801-0387, USA; Leiden University, PO Box 9513, NL-2300, RA Leiden, The Netherlands), AF(CSIRO Astronomy and Space Science (CASS), PO Box 76, Epping, NSW 1710, Australia), AG(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia; ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia), AH(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia), AI(International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia; INAF, Istituto di Radioastronomia, Via Piero Gobetti, I-40129 Bologna, Italy), AJ(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; CSIRO Astronomy and Space Science (CASS), PO Box 76, Epping, NSW 1710, Australia), AK(ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands), AL(Raman Research Institute, Bengaluru 560080, India), AM(International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA 6009, Australia), AN(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands; Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada 0000-0002-3382-9558), AO(International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia), AP(School of Chemical & Physical Sciences, Victoria University of Wellington, Wellington 6140, New Zealand), AQ(International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia), AR(School of Chemical & Physical Sciences, Victoria University of Wellington, Wellington 6140, New Zealand; Peripety Scientific Ltd., PO Box 11355 Manners Street, Wellington 6142, New Zealand), AS(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA 6009, Australia), AT(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006, Australia 0000-0002-9994-1593), AU(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia; ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia), AV(International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia), AW(ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands), AX(ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), School of Physics, The University of Sydney, NSW 2006, Australia; International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA 6009, Australia 0000-0002-8057-0294), AY(International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA 6009, Australia), AZ(School of Chemical & Physical Sciences, Victoria University of Wellington, Wellington 6140, New Zealand; Peripety Scientific Ltd., PO Box 11355 Manners Street, Wellington 6142, New Zealand)
Publication:
Publications of the Astronomical Society of Australia, Volume 34, id.e033 14 pp. (PASA Homepage)
Publication Date:
08/2017
Origin:
CUP
Astronomy Keywords:
Large-scale structure of Universe, radio continuum: galaxies, cosmology: dark ages, reionization, first stars, techniques: interferometric
Abstract Copyright:
2017: Astronomical Society of Australia
DOI:
10.1017/pasa.2017.26
Bibliographic Code:
2017PASA...34...33P

Abstract

The current generation of experiments aiming to detect the neutral hydrogen signal from the Epoch of Reionisation (EoR) is likely to be limited by systematic effects associated with removing foreground sources from target fields. In this paper, we develop a model for the compact foreground sources in one of the target fields of the MWA's EoR key science experiment: the `EoR1' field. The model is based on both the MWA's GLEAM survey and GMRT 150 MHz data from the TGSS survey, the latter providing higher angular resolution and better astrometric accuracy for compact sources than is available from the MWA alone. The model contains 5 049 sources, some of which have complicated morphology in MWA data, Fornax A being the most complex. The higher resolution data show that 13% of sources that appear point-like to the MWA have complicated morphology such as double and quad structure, with a typical separation of 33 arcsec. We derive an analytic expression for the error introduced into the EoR two-dimensional power spectrum due to peeling close double sources as single point sources and show that for the measured source properties, the error in the power spectrum is confined to high k modes that do not affect the overall result for the large-scale cosmological signal of interest. The brightest 10 mis-modelled sources in the field contribute 90% of the power bias in the data, suggesting that it is most critical to improve the models of the brightest sources. With this hybrid model, we reprocess data from the EoR1 field and show a maximum of 8% improved calibration accuracy and a factor of two reduction in residual power in k-space from peeling these sources. Implications for future EoR experiments including the SKA are discussed in relation to the improvements obtained.
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