Journal article

A High-Resolution Foreground Model for the MWA EoR1 Field: Model and Implications for EoR Power Spectrum Analysis

P Procopio, RB Wayth, J Line, CM Trott, HT Intema, DA Mitchell, B Pindor, J Riding, SJ Tingay, ME Bell, JR Callingham, KS Dwarakanath, Bi-Qing For, BM Gaensler, PJ Hancock, L Hindson, N Hurley-Walker, M Johnston-Hollitt, AD Kapinska, E Lenc Show all

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA | CAMBRIDGE UNIV PRESS | Published : 2017

Abstract

AbstractThe 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..

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Grants

Awarded by Australian Research Council's Discovery Early Career Researcher funding scheme


Awarded by Australian Research Council Centre of Excellence


Awarded by Science and Technology Facilities Council


Funding Acknowledgements

CMT is supported under the Australian Research Council's Discovery Early Career Researcher funding scheme (project number DE140100316). The Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020) supported this work. This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the Pawsey Supercomputing Centre that is supported by the Western Australian and Australian Governments. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We acknowledge the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government.