THE MURCHISON WIDEFIELD ARRAY 21 cm POWER SPECTRUM ANALYSIS METHODOLOGY

THE MURCHISON WIDEFIELD ARRAY 21 cm POWER SPECTRUM ANALYSIS METHODOLOGY

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...

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Bibliographic Details
Main Authors: 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., Briggs, F., Cappallo, R. J., Carroll, P., Emrich, D., Gaensler, B. M., Greenhill, L. J., Hurley-Walker, N., Johnston-Hollitt, M., Kaplan, D. L., Kasper, J. C., Kim, H. S., Lenc, E., Line, J., Loeb, A., Lynch, M. J., McKinley, B., Mitchell, D.A., Morales, M. F., Thyagarajan, N., Oberoi, D., Offringa, A. R., Ord, S. M., Paul, S., Prabu, T., Procopio, P., Riding, J., Roshi, A., Shankar, N. Udaya, Sethi, Shiv K., Srivani, K. S., Subrahmanyan, R., Tingay, S. J., Waterson, M., Wayth, R. B., Webster, R. L., Whitney, A. R., Williams, A., Wu, C., Wyithe, J. S. B., Corey, B. E., Kratzenberg, E., Lonsdale, C. J., Rogers, A. E. E., Dillon, Joshua Shane, de Oliveira Costa, Angelica, Ewall-Wice, Aaron Michael, Feng, Lu, Goeke, Robert F, Hewitt, Jacqueline N, Morgan, Edward H, Neben, Abraham Richard, Tegmark, Max Erik, Williams, Christopher Leigh
Other Authors: Haystack Observatory
Format: Article
Language:en_US
Published: IOP Publishing 2016
Online Access:http://hdl.handle.net/1721.1/105094
https://orcid.org/0000-0003-3336-9958
https://orcid.org/0000-0002-0086-7363
https://orcid.org/0000-0003-0422-2324
https://orcid.org/0000-0002-4117-570X
https://orcid.org/0000-0001-7776-7240
https://orcid.org/0000-0001-7670-7190
https://orcid.org/0000-0001-7130-208X
Description
Summary: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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