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    Overcoming real-world obstacles in 21 cm power spectrum estimation: A method demonstration and results from early Murchison Widefield Array data

    245587_195314.pdf (2.283Mb)
    Access Status
    Open access
    Authors
    Dillon, J.
    Liu, A.
    Williams, C.
    Hewit, J.
    Tegmark, M.
    Morgan, E.
    Levine, A.
    Morales, M.
    Tingay, Steven
    BERNARDI, G.
    Bowman, J.
    Briggs, F.
    Cappallo, R.
    Emrich, David
    Mitchell, D.
    Oberoi, D.
    Prabu, T.
    Wayth, Randall
    Webster, R.
    Date
    2014
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Dillon, J. and Liu, A. and Williams, C. and Hewit, J. and Tegmark, M. and Morgan, E. and Levine, A. et al. 2014. Overcoming real-world obstacles in 21 cm power spectrum estimation: A method demonstration and results from early Murchison Widefield Array data. Physical Review D. 89 (2).
    Source Title
    Physical Review D
    DOI
    10.1103/PhysRevD.89.023002
    ISSN
    1550-2368
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    Copyright © 2014 by the American Physical Society

    URI
    http://hdl.handle.net/20.500.11937/23524
    Collection
    • Curtin Research Publications
    Abstract

    We present techniques for bridging the gap between idealized inverse covariance weighted quadratic estimation of 21 cm power spectra and the real-world challenges presented universally by interferometric observation. By carefully evaluating various estimators and adapting our techniques for large but incomplete data sets, we develop a robust power spectrum estimation framework that preserves the so-called "Epoch of Reionization (EoR) window" and keeps track of estimator errors and covariances. We apply our method to observations from the 32-tile prototype of the Murchinson Widefield Array to demonstrate the importance of a judicious analysis technique. Lastly, we apply our method to investigate the dependence of the clean EoR window on frequency—especially the frequency dependence of the so-called “wedge" feature—and establish upper limits on the power spectrum from z ¼ 6.2 to z ¼ 11:7. Our lowest limit is ?ðkÞ < 0.3 Kelvin at 95% confidence at a comoving scale k ¼ 0.046 Mpc-1 and z ¼ 9.5.

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