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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Main Authors:	Jacobs, D., Hazelton, B., Trott, C., Dillon, J., Pindor, B., Sullivan, I., Pober, J., Barry, N., Beardsley, A., Bernardi, G., Bowman, J., Briggs, F., Cappallo, R., Carroll, P., Corey, B., Oliveira-Costa, A., Emrich, D., Ewall-Wice, A., Feng, L., Gaensler, B., Goeke, R., Greenhill, L., Hewitt, J., Hurley-Walker, N., Johnston-Hollitt, M., Kaplan, D., Kasper, J., Kim, H., Kratzenberg, E., Lenc, E., Line, J., Loeb, A., Lonsdale, C., Lynch, M., McKinley, B., McWhirter, S., Mitchell, D., Morales, M., Morgan, E., Neben, A., Thyagarajan, N., Oberoi, D., Offringa, A., Ord, S., Paul, S., Prabu, T., Procopio, P., Riding, J., Rogers, A., Roshi, A., Shankar, N., Sethi, S., Srivani, K., Subrahmanyan, R., Tegmark, M., Tingay, Steven, Waterson, M., Wayth, Randall, Webster, R., Whitney, A., Williams, A., Williams, C., Wu, C., Wyithe, J.
Format:	Journal Article
Published:	Institute of Physics Publishing 2016
Online Access:	http://purl.org/au-research/grants/arc/DE140100316 http://hdl.handle.net/20.500.11937/19602

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author	Jacobs, D. Hazelton, B. Trott, C. Dillon, J. Pindor, B. Sullivan, I. Pober, J. Barry, N. Beardsley, A. Bernardi, G. Bowman, J. Briggs, F. Cappallo, R. Carroll, P. Corey, B. Oliveira-Costa, A. Emrich, D. Ewall-Wice, A. Feng, L. Gaensler, B. Goeke, R. Greenhill, L. Hewitt, J. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. Kasper, J. Kim, H. Kratzenberg, E. Lenc, E. Line, J. Loeb, A. Lonsdale, C. Lynch, M. McKinley, B. McWhirter, S. Mitchell, D. Morales, M. Morgan, E. Neben, A. Thyagarajan, N. Oberoi, D. Offringa, A. Ord, S. Paul, S. Prabu, T. Procopio, P. Riding, J. Rogers, A. Roshi, A. Shankar, N. Sethi, S. Srivani, K. Subrahmanyan, R. Tegmark, M. Tingay, Steven Waterson, M. Wayth, Randall Webster, R. Whitney, A. Williams, A. Williams, C. Wu, C. Wyithe, J.
author_facet	Jacobs, D. Hazelton, B. Trott, C. Dillon, J. Pindor, B. Sullivan, I. Pober, J. Barry, N. Beardsley, A. Bernardi, G. Bowman, J. Briggs, F. Cappallo, R. Carroll, P. Corey, B. Oliveira-Costa, A. Emrich, D. Ewall-Wice, A. Feng, L. Gaensler, B. Goeke, R. Greenhill, L. Hewitt, J. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. Kasper, J. Kim, H. Kratzenberg, E. Lenc, E. Line, J. Loeb, A. Lonsdale, C. Lynch, M. McKinley, B. McWhirter, S. Mitchell, D. Morales, M. Morgan, E. Neben, A. Thyagarajan, N. Oberoi, D. Offringa, A. Ord, S. Paul, S. Prabu, T. Procopio, P. Riding, J. Rogers, A. Roshi, A. Shankar, N. Sethi, S. Srivani, K. Subrahmanyan, R. Tegmark, M. Tingay, Steven Waterson, M. Wayth, Randall Webster, R. Whitney, A. Williams, A. Williams, C. Wu, C. Wyithe, J.
author_sort	Jacobs, D.
building	Curtin Institutional Repository
collection	Online Access
description	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.
first_indexed	2025-11-14T07:31:07Z
format	Journal Article
id	curtin-20.500.11937-19602
institution	Curtin University Malaysia
institution_category	Local University
last_indexed	2025-11-14T07:31:07Z
publishDate	2016
publisher	Institute of Physics Publishing
recordtype	eprints
repository_type	Digital Repository
spelling	curtin-20.500.11937-196022022-09-06T04:20:29Z The murchison widefield array 21 cm power spectrum analysis methodology Jacobs, D. Hazelton, B. Trott, C. Dillon, J. Pindor, B. Sullivan, I. Pober, J. Barry, N. Beardsley, A. Bernardi, G. Bowman, J. Briggs, F. Cappallo, R. Carroll, P. Corey, B. Oliveira-Costa, A. Emrich, D. Ewall-Wice, A. Feng, L. Gaensler, B. Goeke, R. Greenhill, L. Hewitt, J. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. Kasper, J. Kim, H. Kratzenberg, E. Lenc, E. Line, J. Loeb, A. Lonsdale, C. Lynch, M. McKinley, B. McWhirter, S. Mitchell, D. Morales, M. Morgan, E. Neben, A. Thyagarajan, N. Oberoi, D. Offringa, A. Ord, S. Paul, S. Prabu, T. Procopio, P. Riding, J. Rogers, A. Roshi, A. Shankar, N. Sethi, S. Srivani, K. Subrahmanyan, R. Tegmark, M. Tingay, Steven Waterson, M. Wayth, Randall Webster, R. Whitney, A. Williams, A. Williams, C. Wu, C. Wyithe, J. 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. 2016 Journal Article http://hdl.handle.net/20.500.11937/19602 10.3847/0004-637X/825/2/114 http://purl.org/au-research/grants/arc/DE140100316 Institute of Physics Publishing fulltext
spellingShingle	Jacobs, D. Hazelton, B. Trott, C. Dillon, J. Pindor, B. Sullivan, I. Pober, J. Barry, N. Beardsley, A. Bernardi, G. Bowman, J. Briggs, F. Cappallo, R. Carroll, P. Corey, B. Oliveira-Costa, A. Emrich, D. Ewall-Wice, A. Feng, L. Gaensler, B. Goeke, R. Greenhill, L. Hewitt, J. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. Kasper, J. Kim, H. Kratzenberg, E. Lenc, E. Line, J. Loeb, A. Lonsdale, C. Lynch, M. McKinley, B. McWhirter, S. Mitchell, D. Morales, M. Morgan, E. Neben, A. Thyagarajan, N. Oberoi, D. Offringa, A. Ord, S. Paul, S. Prabu, T. Procopio, P. Riding, J. Rogers, A. Roshi, A. Shankar, N. Sethi, S. Srivani, K. Subrahmanyan, R. Tegmark, M. Tingay, Steven Waterson, M. Wayth, Randall Webster, R. Whitney, A. Williams, A. Williams, C. Wu, C. Wyithe, J. The murchison widefield array 21 cm power spectrum analysis methodology
title	The murchison widefield array 21 cm power spectrum analysis methodology
title_full	The murchison widefield array 21 cm power spectrum analysis methodology
title_fullStr	The murchison widefield array 21 cm power spectrum analysis methodology
title_full_unstemmed	The murchison widefield array 21 cm power spectrum analysis methodology
title_short	The murchison widefield array 21 cm power spectrum analysis methodology
title_sort	murchison widefield array 21 cm power spectrum analysis methodology
url	http://purl.org/au-research/grants/arc/DE140100316 http://hdl.handle.net/20.500.11937/19602

The murchison widefield array 21 cm power spectrum analysis methodology

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