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    The murchison widefield array 21 cm power spectrum analysis methodology

    241756_241756.pdf (9.306Mb)
    Access Status
    Open access
    Authors
    Jacobs, D.
    Hazelton, B.
    Trott, C.
    Dillon, J.
    Pindor, B.
    Sullivan, I.
    Pober, J.
    Barry, N.
    Beardsley, A.
    Bernardi, G.
    Bowman, J.
    Briggs, F.
    Cappallo, R.
    Carroll, P.
    Corey, B.
    Oliveira-Costa, A.
    Emrich, D.
    Ewall-Wice, A.
    Feng, L.
    Gaensler, B.
    Goeke, R.
    Greenhill, L.
    Hewitt, J.
    Hurley-Walker, N.
    Johnston-Hollitt, M.
    Kaplan, D.
    Kasper, J.
    Kim, H.
    Kratzenberg, E.
    Lenc, E.
    Line, J.
    Loeb, A.
    Lonsdale, C.
    Lynch, M.
    McKinley, B.
    McWhirter, S.
    Mitchell, D.
    Morales, M.
    Morgan, E.
    Neben, A.
    Thyagarajan, N.
    Oberoi, D.
    Offringa, A.
    Ord, S.
    Paul, S.
    Prabu, T.
    Procopio, P.
    Riding, J.
    Rogers, A.
    Roshi, A.
    Shankar, N.
    Sethi, S.
    Srivani, K.
    Subrahmanyan, R.
    Tegmark, M.
    Tingay, Steven
    Waterson, M.
    Wayth, Randall
    Webster, R.
    Whitney, A.
    Williams, A.
    Williams, C.
    Wu, C.
    Wyithe, J.
    Date
    2016
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Jacobs, D. and Hazelton, B. and Trott, C. and Dillon, J. and Pindor, B. and Sullivan, I. and Pober, J. et al. 2016. The murchison widefield array 21 cm power spectrum analysis methodology. Astrophysical Journal. 825 (2): Article ID 114.
    Source Title
    Astrophysical Journal
    DOI
    10.3847/0004-637X/825/2/114
    ISSN
    0004-637X
    School
    Curtin Institute of Radio Astronomy (Physics)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/DE140100316
    URI
    http://hdl.handle.net/20.500.11937/19602
    Collection
    • Curtin Research Publications
    Abstract

    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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