The murchison widefield array 21 cm power spectrum analysis methodology

Daniel Jacobs; B. J. Hazelton; C. M. Trott; Joshua S. Dillon; B. Pindor; I. S. Sullivan; J. C. Pober; N. Barry; A. P. Beardsley; G. Bernardi; Judd Bowman; F. Briggs; R. J. Cappallo; P. Carroll; B. E. Corey; A. De 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; Hs 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. Udaya Shankar; Shiv 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; C. Wu; J. S B Wyithe

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

The murchison widefield array 21 cm power spectrum analysis methodology

Daniel Jacobs, B. J. Hazelton, C. M. Trott, Joshua S. Dillon, B. Pindor, I. S. Sullivan, J. C. Pober, N. Barry, A. P. Beardsley, G. Bernardi, Judd Bowman, F. Briggs, R. J. Cappallo, P. Carroll, B. E. Corey, A. De 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, Hs 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. Udaya Shankar, Shiv 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, C. Wu, J. S B Wyithe

Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Article › peer-review

68 Scopus citations

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.

Original language	English (US)
Article number	114
Journal	Astrophysical Journal
Volume	825
Issue number	2
DOIs	https://doi.org/10.3847/0004-637X/825/2/114
State	Published - Jul 10 2016

Keywords

dark ages, reionization, first stars
methods: data analysis
techniques: interferometric

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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

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Jacobs, D., 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., 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. Astrophysical Journal, 825(2), Article 114. https://doi.org/10.3847/0004-637X/825/2/114

Jacobs, D, Hazelton, BJ, Trott, CM, Dillon, JS, Pindor, B, Sullivan, IS, Pober, JC, Barry, N, Beardsley, AP, Bernardi, G, Bowman, J, 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', Astrophysical Journal, vol. 825, no. 2, 114. https://doi.org/10.3847/0004-637X/825/2/114

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

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AU - Jacobs, Daniel

AU - Hazelton, B. J.

AU - Trott, C. M.

AU - Dillon, Joshua S.

AU - Pindor, B.

AU - Sullivan, I. S.

AU - Pober, J. C.

AU - Barry, N.

AU - Beardsley, A. P.

AU - Bernardi, G.

AU - Bowman, Judd

AU - Briggs, F.

AU - Cappallo, R. J.

AU - Carroll, P.

AU - Corey, B. E.

AU - Oliveira-Costa, A. De

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, Hs

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. Udaya

AU - Sethi, Shiv 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, C.

AU - Wyithe, J. S B

PY - 2016/7/10

Y1 - 2016/7/10

N2 - 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 - 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.

KW - dark ages, reionization, first stars

KW - methods: data analysis

KW - techniques: interferometric

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

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VL - 825

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 114

ER -

The murchison widefield array 21 cm power spectrum analysis methodology

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Keywords

ASJC Scopus subject areas

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