The murchison widefield array 21 cm power spectrum analysis methodology

D.C. Jacobs; B.J. Hazelton; C.M. Trott; J.S. Dillon; B. Pindor; I.S. Sullivan; J.C. Pober; N. Barry; A.P. Beardsley; G. Bernardi; J.D. Bowman; F. Briggs; R.J. Cappallo; P. Carroll; B.E. Corey; A.D. 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. 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.U. Shankar; S.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; Chen Wu; J.S.B. Wyithe

doi:10.3847/0004-637X/825/2/114

The murchison widefield array 21 cm power spectrum analysis methodology

D.C. Jacobs, B.J. Hazelton, C.M. Trott, J.S. Dillon, B. Pindor, I.S. Sullivan, J.C. Pober, N. Barry, A.P. Beardsley, G. Bernardi, J.D. Bowman, F. Briggs, R.J. Cappallo, P. Carroll, B.E. Corey, A.D. Oliveira-Costa, D. Emrich, A. Ewall-Wice, L. Feng, B.M. GaenslerR. Goeke, L.J. Greenhill, J.N. Hewitt, N. Hurley-Walker, M. Johnston-Hollitt, D.L. Kaplan, J.C. Kasper, H. 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.U. Shankar, S.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, Chen Wu, J.S.B. Wyithe

International Centre for Radio Astronomy Research (ICRAR)

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Abstract

© 2016. The American Astronomical Society. All rights reserved.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.

Original language	English
Article number	114
Pages (from-to)	1-16
Journal	The Astrophysical Journal
Volume	825
Issue number	2
DOIs	https://doi.org/10.3847/0004-637X/825/2/114
Publication status	Published - 10 Jul 2016

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10.3847/0004-637X/825/2/114

Jacobs et al., 2016 THE MURCHISON WIDEFIELD ARRAY 21 cm POWER SPECTRUM ANALYSIS METHODOLOGYFinal published version, 7.72 MBLicence: Unspecified

MIRA Widefield Array - A New Low Frequency Telescope
Staveley-Smith, L., Webster, R., Briggs, F., Dickey, J., Lynch, M., Green, A., Bailes, M., Lonsdale, C., Boyle, B., Greenhill, L. & Sault, R.
ARC Australian Research Council
1/01/08 → 31/12/09
Project: Research

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Jacobs, D. C., Hazelton, B. J., Trott, C. M., Dillon, J. S., Pindor, B., Sullivan, I. S., Pober, J. C., Barry, N., Beardsley, A. P., Bernardi, G., Bowman, J. D., Briggs, F., Cappallo, R. J., Carroll, P., Corey, B. E., Oliveira-Costa, A. D., Emrich, D., Ewall-Wice, A., Feng, L., ... Wyithe, J. S. B. (2016). The murchison widefield array 21 cm power spectrum analysis methodology. The Astrophysical Journal, 825(2), 1-16. Article 114. https://doi.org/10.3847/0004-637X/825/2/114

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title = "The murchison widefield array 21 cm power spectrum analysis methodology",

abstract = "{\textcopyright} 2016. The American Astronomical Society. All rights reserved.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.",

author = "D.C. Jacobs and B.J. Hazelton and C.M. Trott and J.S. Dillon and B. Pindor and I.S. Sullivan and J.C. Pober and N. Barry and A.P. Beardsley and G. Bernardi and J.D. Bowman and F. Briggs and R.J. Cappallo and P. Carroll and B.E. Corey and A.D. Oliveira-Costa and D. Emrich and A. Ewall-Wice and L. Feng and B.M. Gaensler and R. Goeke and L.J. Greenhill and J.N. Hewitt and N. Hurley-Walker and M. Johnston-Hollitt and D.L. Kaplan and J.C. Kasper and H. Kim and E. Kratzenberg and E. Lenc and J. Line and A. Loeb and C.J. Lonsdale and M.J. Lynch and B. Mckinley and S.R. Mcwhirter and D.A. Mitchell and M.F. Morales and E. Morgan and A.R. Neben and N. Thyagarajan and D. Oberoi and A.R. Offringa and S.M. Ord and S. Paul and T. Prabu and P. Procopio and J. Riding and A.E.E. Rogers and A. Roshi and N.U. Shankar and S.K. Sethi and K.S. Srivani and R. Subrahmanyan and M. Tegmark and S.J. Tingay and M. Waterson and R.B. Wayth and R.L. Webster and A.R. Whitney and A. Williams and C.L. Williams and Chen Wu and J.S.B. Wyithe",

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journal = "The Astrophysical Journal",

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Jacobs, DC, Hazelton, BJ, Trott, CM, Dillon, JS, Pindor, B, Sullivan, IS, Pober, JC, Barry, N, Beardsley, AP, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Carroll, P, Corey, BE, Oliveira-Costa, AD, Emrich, D, Ewall-Wice, A, Feng, L, Gaensler, BM, Goeke, R, Greenhill, LJ, Hewitt, JN, Hurley-Walker, N, Johnston-Hollitt, M, Kaplan, DL, Kasper, JC, Kim, H, Kratzenberg, E, Lenc, E, Line, J, Loeb, A, Lonsdale, CJ, Lynch, MJ, Mckinley, B, Mcwhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Neben, AR, Thyagarajan, N, Oberoi, D, Offringa, AR, Ord, SM, Paul, S, Prabu, T, Procopio, P, Riding, J, Rogers, AEE, Roshi, A, Shankar, NU, Sethi, SK, Srivani, KS, Subrahmanyan, R, Tegmark, M, Tingay, SJ, Waterson, M, Wayth, RB, Webster, RL, Whitney, AR, Williams, A, Williams, CL, Wu, C & Wyithe, JSB 2016, 'The murchison widefield array 21 cm power spectrum analysis methodology', The Astrophysical Journal, vol. 825, no. 2, 114, pp. 1-16. https://doi.org/10.3847/0004-637X/825/2/114

TY - JOUR

T1 - The murchison widefield array 21 cm power spectrum analysis methodology

AU - Jacobs, D.C.

AU - Hazelton, B.J.

AU - Trott, C.M.

AU - Dillon, J.S.

AU - Pindor, B.

AU - Sullivan, I.S.

AU - Pober, J.C.

AU - Barry, N.

AU - Beardsley, A.P.

AU - Bernardi, G.

AU - Bowman, J.D.

AU - Briggs, F.

AU - Cappallo, R.J.

AU - Carroll, P.

AU - Corey, B.E.

AU - Oliveira-Costa, A.D.

AU - Emrich, D.

AU - Ewall-Wice, A.

AU - Feng, L.

AU - Gaensler, B.M.

AU - Goeke, R.

AU - Greenhill, L.J.

AU - Hewitt, J.N.

AU - Hurley-Walker, N.

AU - Johnston-Hollitt, M.

AU - Kaplan, D.L.

AU - Kasper, J.C.

AU - Kim, H.

AU - Kratzenberg, E.

AU - Lenc, E.

AU - Line, J.

AU - Loeb, A.

AU - Lonsdale, C.J.

AU - Lynch, M.J.

AU - Mckinley, B.

AU - Mcwhirter, S.R.

AU - Mitchell, D.A.

AU - Morales, M.F.

AU - Morgan, E.

AU - Neben, A.R.

AU - Thyagarajan, N.

AU - Oberoi, D.

AU - Offringa, A.R.

AU - Ord, S.M.

AU - Paul, S.

AU - Prabu, T.

AU - Procopio, P.

AU - Riding, J.

AU - Rogers, A.E.E.

AU - Roshi, A.

AU - Shankar, N.U.

AU - Sethi, S.K.

AU - Srivani, K.S.

AU - Subrahmanyan, R.

AU - Tegmark, M.

AU - Tingay, S.J.

AU - Waterson, M.

AU - Wayth, R.B.

AU - Webster, R.L.

AU - Whitney, A.R.

AU - Williams, A.

AU - Williams, C.L.

AU - Wu, Chen

AU - Wyithe, J.S.B.

PY - 2016/7/10

Y1 - 2016/7/10

N2 - © 2016. The American Astronomical Society. All rights reserved.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.

AB - © 2016. The American Astronomical Society. All rights reserved.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.

U2 - 10.3847/0004-637X/825/2/114

DO - 10.3847/0004-637X/825/2/114

M3 - Article

SN - 0004-637X

VL - 825

SP - 1

EP - 16

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 2

M1 - 114

ER -

The murchison widefield array 21 cm power spectrum analysis methodology

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