FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7

A. P. Beardsley; B. J. Hazelton; I. S. Sullivan; P. Carroll; N. Barry; M. Rahimi; B. Pindor; C. M. Trott; J. Line; Daniel C. Jacobs; M. F. Morales; J. C. Pober; G. Bernardi; Judd D. Bowman; M. P. Busch; F. Briggs; R. J. Cappallo; B. E. Corey; A. De Oliveira-Costa; Joshua S. Dillon; 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. S. Kim; E. Kratzenberg; E. Lenc; A. Loeb; C. J. Lonsdale; M. J. Lynch; B. McKinley; S. R. McWhirter; D. A. Mitchell; E. Morgan; A. R. Neben; Nithyanandan 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:10.3847/1538-4357/833/1/102

FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7

A. P. Beardsley, B. J. Hazelton, I. S. Sullivan, P. Carroll, N. Barry, M. Rahimi, B. Pindor, C. M. Trott, J. Line, Daniel C. Jacobs, M. F. Morales, J. C. Pober, G. Bernardi, Judd D. Bowman, M. P. Busch, F. Briggs, R. J. Cappallo, B. E. Corey, A. De Oliveira-Costa, Joshua S. DillonD. 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. S. Kim, E. Kratzenberg, E. Lenc, A. Loeb, C. J. Lonsdale, M. J. Lynch, B. McKinley, S. R. McWhirter, D. A. Mitchell, E. Morgan, A. R. Neben, Nithyanandan 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

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Abstract

The Murchison Widefield Array (MWA) has collected hundreds of hours of Epoch of Reionization (EoR) data andnow faces the challenge of overcoming foreground and systematic contamination to reduce the data to acosmological measurement. We introduce several novel analysis techniques, such as cable reflection calibration,hyper-resolution gridding kernels, diffuse foreground model subtraction, and quality control methods. Each changeto the analysis pipeline is tested against a two-dimensional power spectrum figure of merit to demonstrateimprovement. We incorporate the new techniques into a deep integration of 32 hours of MWA data. This data set isused to place a systematic-limited upper limit on the cosmological power spectrum of Δ² ≤ 2.7×10⁴ mK² at k =0.27 h Mpc^-1 and z = 7.1, consistent with other published limits, and a modest improvement (factor of 1.4) overprevious MWA results. From this deep analysis, we have identified a list of improvements to be made to our EoRdata analysis strategies. These improvements will be implemented in the future and detailed in upcomingpublications.

Original language	English
Article number	102
Journal	Astrophysical Journal
Volume	833
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/833/1/102
Publication status	Published - 10 Dec 2016

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Beardsley, A. P., Hazelton, B. J., Sullivan, I. S., Carroll, P., Barry, N., Rahimi, M., Pindor, B., Trott, C. M., Line, J., Jacobs, D. C., Morales, M. F., Pober, J. C., Bernardi, G., Bowman, J. D., Busch, M. P., Briggs, F., Cappallo, R. J., Corey, B. E., Oliveira-Costa, A. D., ... Wyithe, J. S. B. (2016). FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7. Astrophysical Journal, 833(1), Article 102. https://doi.org/10.3847/1538-4357/833/1/102

@article{508fbf8f798d4b51a15c182e819fe58d,

title = "FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7",

abstract = "The Murchison Widefield Array (MWA) has collected hundreds of hours of Epoch of Reionization (EoR) data andnow faces the challenge of overcoming foreground and systematic contamination to reduce the data to acosmological measurement. We introduce several novel analysis techniques, such as cable reflection calibration,hyper-resolution gridding kernels, diffuse foreground model subtraction, and quality control methods. Each changeto the analysis pipeline is tested against a two-dimensional power spectrum figure of merit to demonstrateimprovement. We incorporate the new techniques into a deep integration of 32 hours of MWA data. This data set isused to place a systematic-limited upper limit on the cosmological power spectrum of Δ2 ≤ 2.7×104 mK2 at k =0.27 h Mpc-1 and z = 7.1, consistent with other published limits, and a modest improvement (factor of 1.4) overprevious MWA results. From this deep analysis, we have identified a list of improvements to be made to our EoRdata analysis strategies. These improvements will be implemented in the future and detailed in upcomingpublications.",

keywords = "cosmology: observations, cosmology: reionization",

author = "Beardsley, {A. P.} and Hazelton, {B. J.} and Sullivan, {I. S.} and P. Carroll and N. Barry and M. Rahimi and B. Pindor and Trott, {C. M.} and J. Line and Jacobs, {Daniel C.} and Morales, {M. F.} and Pober, {J. C.} and G. Bernardi and Bowman, {Judd D.} and Busch, {M. P.} and F. Briggs and Cappallo, {R. J.} and Corey, {B. E.} and Oliveira-Costa, {A. De} and Dillon, {Joshua S.} 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 Kim, {H. S.} and E. Kratzenberg and E. Lenc and A. Loeb and Lonsdale, {C. J.} and Lynch, {M. J.} and B. McKinley and McWhirter, {S. R.} and Mitchell, {D. A.} and E. Morgan and Neben, {A. R.} and Nithyanandan 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.}",

year = "2016",

month = dec,

day = "10",

doi = "10.3847/1538-4357/833/1/102",

language = "English",

volume = "833",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Beardsley, AP, Hazelton, BJ, Sullivan, IS, Carroll, P, Barry, N, Rahimi, M, Pindor, B, Trott, CM, Line, J, Jacobs, DC, Morales, MF, Pober, JC, Bernardi, G, Bowman, JD, Busch, MP, Briggs, F, Cappallo, RJ, Corey, BE, Oliveira-Costa, AD, Dillon, JS, 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, HS, Kratzenberg, E, Lenc, E, Loeb, A, Lonsdale, CJ, Lynch, MJ, McKinley, B, McWhirter, SR, Mitchell, DA, 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, 'FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7', Astrophysical Journal, vol. 833, no. 1, 102. https://doi.org/10.3847/1538-4357/833/1/102

TY - JOUR

T1 - FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7

AU - Beardsley, A. P.

AU - Hazelton, B. J.

AU - Sullivan, I. S.

AU - Carroll, P.

AU - Barry, N.

AU - Rahimi, M.

AU - Pindor, B.

AU - Trott, C. M.

AU - Line, J.

AU - Jacobs, Daniel C.

AU - Morales, M. F.

AU - Pober, J. C.

AU - Bernardi, G.

AU - Bowman, Judd D.

AU - Busch, M. P.

AU - Briggs, F.

AU - Cappallo, R. J.

AU - Corey, B. E.

AU - Oliveira-Costa, A. De

AU - Dillon, Joshua S.

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. S.

AU - Kratzenberg, E.

AU - Lenc, E.

AU - Loeb, A.

AU - Lonsdale, C. J.

AU - Lynch, M. J.

AU - McKinley, B.

AU - McWhirter, S. R.

AU - Mitchell, D. A.

AU - Morgan, E.

AU - Neben, A. R.

AU - Thyagarajan, Nithyanandan

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 - 2016/12/10

Y1 - 2016/12/10

N2 - The Murchison Widefield Array (MWA) has collected hundreds of hours of Epoch of Reionization (EoR) data andnow faces the challenge of overcoming foreground and systematic contamination to reduce the data to acosmological measurement. We introduce several novel analysis techniques, such as cable reflection calibration,hyper-resolution gridding kernels, diffuse foreground model subtraction, and quality control methods. Each changeto the analysis pipeline is tested against a two-dimensional power spectrum figure of merit to demonstrateimprovement. We incorporate the new techniques into a deep integration of 32 hours of MWA data. This data set isused to place a systematic-limited upper limit on the cosmological power spectrum of Δ2 ≤ 2.7×104 mK2 at k =0.27 h Mpc-1 and z = 7.1, consistent with other published limits, and a modest improvement (factor of 1.4) overprevious MWA results. From this deep analysis, we have identified a list of improvements to be made to our EoRdata analysis strategies. These improvements will be implemented in the future and detailed in upcomingpublications.

AB - The Murchison Widefield Array (MWA) has collected hundreds of hours of Epoch of Reionization (EoR) data andnow faces the challenge of overcoming foreground and systematic contamination to reduce the data to acosmological measurement. We introduce several novel analysis techniques, such as cable reflection calibration,hyper-resolution gridding kernels, diffuse foreground model subtraction, and quality control methods. Each changeto the analysis pipeline is tested against a two-dimensional power spectrum figure of merit to demonstrateimprovement. We incorporate the new techniques into a deep integration of 32 hours of MWA data. This data set isused to place a systematic-limited upper limit on the cosmological power spectrum of Δ2 ≤ 2.7×104 mK2 at k =0.27 h Mpc-1 and z = 7.1, consistent with other published limits, and a modest improvement (factor of 1.4) overprevious MWA results. From this deep analysis, we have identified a list of improvements to be made to our EoRdata analysis strategies. These improvements will be implemented in the future and detailed in upcomingpublications.

KW - cosmology: observations

KW - cosmology: reionization

UR - http://www.scopus.com/inward/record.url?scp=85006381038&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/833/1/102

DO - 10.3847/1538-4357/833/1/102

M3 - Article

SN - 0004-637X

VL - 833

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 102

ER -

FIRST SEASON MWA EOR POWER SPECTRUM RESULTS at REDSHIFT 7

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