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arxiv 1605.06978 v1 pith:43SC4VOT submitted 2016-05-23 astro-ph.IM astro-ph.CO

The Murchison Widefield Array 21 cm Power Spectrum Analysis Methodology

Daniel C. Jacobs , B. J. Hazelton , C. M. Trott , Joshua S. Dillon , B. Pindor , I. S. Sullivan , J. C. Pober , N. Barry
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A. P. Beardsley G. Bernardi Judd D. Bowman F. Briggs R. J. Cappallo P. Carroll B. E. Corey A. de Oliveira-Costa D. Emrich A. Ewall-Wice L. Feng B. M. Gaensler R. Goeke L. J. Greenhill J. N. Hewitt N. Hurley-Walker M. Johnston-Hollitt D. L. Kaplan J. C. Kasper H. S. Kim E. Kratzenberg E. Lenc J. Line A. Loeb C. J. Lonsdale M. J. Lynch B. McKinley S. R. McWhirter D. A. Mitchell M. F. Morales E. Morgan A. R. Neben N. Thyagarajan D. Oberoi A. R. Offringa S. M. Ord S. Paul T. Prabu P. Procopio J. Riding A. E. E. Rogers A. Roshi N. Udaya Shankar Shiv K. Sethi K. S. Srivani R. Subrahmanyan M. Tegmark S. J. Tingay M. Waterson R. B. Wayth R. L. Webster A. R. Whitney A. Williams C. L. Williams C. Wu J. S. B. Wyithe
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classification astro-ph.IM astro-ph.CO
keywords powerspectrumpipelinesanalysisarraycalibrationcomparingdata
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We present the 21 cm power spectrum analysis approach of the Murchison Widefield Array Epoch of Reionization project. In this paper, we compare the outputs of multiple pipelines for the purpose of validating statistical limits cosmological hydrogen at redshifts between 6 and 12. Multiple, independent, data calibration and reduction pipelines are used to make power spectrum limits on a fiducial night of data. Comparing the outputs of imaging and power spectrum stages highlights differences in calibration, foreground subtraction and power spectrum calculation. The power spectra found using these different methods span a space defined by the various tradeoffs between speed, accuracy, and systematic control. Lessons learned from comparing the pipelines range from the algorithmic to the prosaically mundane; all demonstrate the many pitfalls of neglecting reproducibility. We briefly discuss the way these different methods attempt to handle the question of evaluating a significant detection in the presence of foregrounds.

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  1. Observations of the Cosmic Dawn and Epoch of Reionization with the SKAO: Observational Lessons Learned from Precursors and Pathfinder Instruments

    astro-ph.IM 2026-06 unverdicted novelty 2.0

    Summarizes observational lessons on simulation pipelines and systematic mitigation from SKAO precursors for Cosmic Dawn and EoR studies.