THE MURCHISON WIDEFIELD ARRAY 21 cm POWER SPECTRUM ANALYSIS METHODOLOGY
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Jacobs-2016-THE MURCHISON WIDEFI.pdf
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7.72 MB
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Author(s)
Jacobs, Daniel C.
Hazelton, B. J.
Trott, C. M.
Pindor, B.
Sullivan, I. S.
Pober, J. C.
Barry, N.
Beardsley, A. P.
Bernardi, G.
Bowman, Judd D.
Date Issued
July 2016
Journal
Astrophysical Journal
Publisher
IOP Publishing
Citation
Jacobs, Daniel C., B. J. Hazelton, C. M. Trott, Joshua S. Dillon, B. Pindor, I. S. Sullivan, J. C. Pober, et al. “THE MURCHISON WIDEFIELD ARRAY 21 Cm POWER SPECTRUM ANALYSIS METHODOLOGY.” The Astrophysical Journal vol. 825, no. 2, 114, July 2016, pp. 1-16. © 2016. The American Astronomical Society.
Version
Final published version
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.
MIT Department
Haystack Observatory
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.3847/0004-637x/825/2/114
