Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al.

Joshua S. Dillon, Abraham R. Neben, Jacqueline N. Hewitt, Max Tegmark, N. Barry, A. P. Beardsley, Judd Bowman, F. Briggs, P. Carroll, A. De Oliveira-Costa, A. Ewall-Wice, L. Feng, L. J. Greenhill, B. J. Hazelton, L. Hernquist, N. Hurley-Walker, Daniel Jacobs, H. S. Kim, P. Kittiwisit, E. LencJ. Line, A. Loeb, B. McKinley, D. A. Mitchell, M. F. Morales, A. R. Offringa, S. Paul, B. Pindor, J. C. Pober, P. Procopio, J. Riding, S. Sethi, N. Udaya Shankar, R. Subrahmanyan, I. Sullivan, Nithyanandan Thyagarajan, S. J. Tingay, C. Trott, R. B. Wayth, R. L. Webster, S. Wyithe, G. Bernardi, R. J. Cappallo, A. A. Deshpande, M. Johnston-Hollitt, D. L. Kaplan, C. J. Lonsdale, S. R. McWhirter, E. Morgan, D. Oberoi, S. M. Ord, T. Prabu, K. S. Srivani, A. Williams, C. L. Williams

Research output: Contribution to journalArticle

60 Citations (Scopus)

Abstract

The separation of the faint cosmological background signal from bright astrophysical foregrounds remains one of the most daunting challenges of mapping the high-redshift intergalactic medium with the redshifted 21 cm line of neutral hydrogen. Advances in mapping and modeling of diffuse and point source foregrounds have improved subtraction accuracy, but no subtraction scheme is perfect. Precisely quantifying the errors and error correlations due to missubtracted foregrounds allows for both the rigorous analysis of the 21 cm power spectrum and for the maximal isolation of the "EoR window" from foreground contamination. We present a method to infer the covariance of foreground residuals from the data itself in contrast to previous attempts at a priori modeling. We demonstrate our method by setting limits on the power spectrum using a 3 h integration from the 128-tile Murchison Widefield Array. Observing between 167 and 198 MHz, we find at 95% confidence a best limit of Δ2(k)

Original languageEnglish (US)
Article number123011
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume91
Issue number12
DOIs
StatePublished - Jun 19 2015

Fingerprint

tiles
subtraction
power spectra
intergalactic media
point sources
confidence
isolation
astrophysics
contamination
hydrogen

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Empirical covariance modeling for 21 cm power spectrum estimation : A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al. / Dillon, Joshua S.; Neben, Abraham R.; Hewitt, Jacqueline N.; Tegmark, Max; Barry, N.; Beardsley, A. P.; Bowman, Judd; Briggs, F.; Carroll, P.; De Oliveira-Costa, A.; Ewall-Wice, A.; Feng, L.; Greenhill, L. J.; Hazelton, B. J.; Hernquist, L.; Hurley-Walker, N.; Jacobs, Daniel; Kim, H. S.; Kittiwisit, P.; Lenc, E.; Line, J.; Loeb, A.; McKinley, B.; Mitchell, D. A.; Morales, M. F.; Offringa, A. R.; Paul, S.; Pindor, B.; Pober, J. C.; Procopio, P.; Riding, J.; Sethi, S.; Shankar, N. Udaya; Subrahmanyan, R.; Sullivan, I.; Thyagarajan, Nithyanandan; Tingay, S. J.; Trott, C.; Wayth, R. B.; Webster, R. L.; Wyithe, S.; Bernardi, G.; Cappallo, R. J.; Deshpande, A. A.; Johnston-Hollitt, M.; Kaplan, D. L.; Lonsdale, C. J.; McWhirter, S. R.; Morgan, E.; Oberoi, D.; Ord, S. M.; Prabu, T.; Srivani, K. S.; Williams, A.; Williams, C. L.

In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 91, No. 12, 123011, 19.06.2015.

Research output: Contribution to journalArticle

Dillon, JS, Neben, AR, Hewitt, JN, Tegmark, M, Barry, N, Beardsley, AP, Bowman, J, Briggs, F, Carroll, P, De Oliveira-Costa, A, Ewall-Wice, A, Feng, L, Greenhill, LJ, Hazelton, BJ, Hernquist, L, Hurley-Walker, N, Jacobs, D, Kim, HS, Kittiwisit, P, Lenc, E, Line, J, Loeb, A, McKinley, B, Mitchell, DA, Morales, MF, Offringa, AR, Paul, S, Pindor, B, Pober, JC, Procopio, P, Riding, J, Sethi, S, Shankar, NU, Subrahmanyan, R, Sullivan, I, Thyagarajan, N, Tingay, SJ, Trott, C, Wayth, RB, Webster, RL, Wyithe, S, Bernardi, G, Cappallo, RJ, Deshpande, AA, Johnston-Hollitt, M, Kaplan, DL, Lonsdale, CJ, McWhirter, SR, Morgan, E, Oberoi, D, Ord, SM, Prabu, T, Srivani, KS, Williams, A & Williams, CL 2015, 'Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al.', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 91, no. 12, 123011. https://doi.org/10.1103/PhysRevD.91.123011
Dillon, Joshua S. ; Neben, Abraham R. ; Hewitt, Jacqueline N. ; Tegmark, Max ; Barry, N. ; Beardsley, A. P. ; Bowman, Judd ; Briggs, F. ; Carroll, P. ; De Oliveira-Costa, A. ; Ewall-Wice, A. ; Feng, L. ; Greenhill, L. J. ; Hazelton, B. J. ; Hernquist, L. ; Hurley-Walker, N. ; Jacobs, Daniel ; Kim, H. S. ; Kittiwisit, P. ; Lenc, E. ; Line, J. ; Loeb, A. ; McKinley, B. ; Mitchell, D. A. ; Morales, M. F. ; Offringa, A. R. ; Paul, S. ; Pindor, B. ; Pober, J. C. ; Procopio, P. ; Riding, J. ; Sethi, S. ; Shankar, N. Udaya ; Subrahmanyan, R. ; Sullivan, I. ; Thyagarajan, Nithyanandan ; Tingay, S. J. ; Trott, C. ; Wayth, R. B. ; Webster, R. L. ; Wyithe, S. ; Bernardi, G. ; Cappallo, R. J. ; Deshpande, A. A. ; Johnston-Hollitt, M. ; Kaplan, D. L. ; Lonsdale, C. J. ; McWhirter, S. R. ; Morgan, E. ; Oberoi, D. ; Ord, S. M. ; Prabu, T. ; Srivani, K. S. ; Williams, A. ; Williams, C. L. / Empirical covariance modeling for 21 cm power spectrum estimation : A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al. In: Physical Review D - Particles, Fields, Gravitation and Cosmology. 2015 ; Vol. 91, No. 12.
@article{f922117713724b3f828ab831f224fda1,
title = "Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al.",
abstract = "The separation of the faint cosmological background signal from bright astrophysical foregrounds remains one of the most daunting challenges of mapping the high-redshift intergalactic medium with the redshifted 21 cm line of neutral hydrogen. Advances in mapping and modeling of diffuse and point source foregrounds have improved subtraction accuracy, but no subtraction scheme is perfect. Precisely quantifying the errors and error correlations due to missubtracted foregrounds allows for both the rigorous analysis of the 21 cm power spectrum and for the maximal isolation of the {"}EoR window{"} from foreground contamination. We present a method to infer the covariance of foreground residuals from the data itself in contrast to previous attempts at a priori modeling. We demonstrate our method by setting limits on the power spectrum using a 3 h integration from the 128-tile Murchison Widefield Array. Observing between 167 and 198 MHz, we find at 95{\%} confidence a best limit of Δ2(k)",
author = "Dillon, {Joshua S.} and Neben, {Abraham R.} and Hewitt, {Jacqueline N.} and Max Tegmark and N. Barry and Beardsley, {A. P.} and Judd Bowman and F. Briggs and P. Carroll and {De Oliveira-Costa}, A. and A. Ewall-Wice and L. Feng and Greenhill, {L. J.} and Hazelton, {B. J.} and L. Hernquist and N. Hurley-Walker and Daniel Jacobs and Kim, {H. S.} and P. Kittiwisit and E. Lenc and J. Line and A. Loeb and B. McKinley and Mitchell, {D. A.} and Morales, {M. F.} and Offringa, {A. R.} and S. Paul and B. Pindor and Pober, {J. C.} and P. Procopio and J. Riding and S. Sethi and Shankar, {N. Udaya} and R. Subrahmanyan and I. Sullivan and Nithyanandan Thyagarajan and Tingay, {S. J.} and C. Trott and Wayth, {R. B.} and Webster, {R. L.} and S. Wyithe and G. Bernardi and Cappallo, {R. J.} and Deshpande, {A. A.} and M. Johnston-Hollitt and Kaplan, {D. L.} and Lonsdale, {C. J.} and McWhirter, {S. R.} and E. Morgan and D. Oberoi and Ord, {S. M.} and T. Prabu and Srivani, {K. S.} and A. Williams and Williams, {C. L.}",
year = "2015",
month = "6",
day = "19",
doi = "10.1103/PhysRevD.91.123011",
language = "English (US)",
volume = "91",
journal = "Physical review D: Particles and fields",
issn = "1550-7998",
publisher = "American Institute of Physics Publising LLC",
number = "12",

}

TY - JOUR

T1 - Empirical covariance modeling for 21 cm power spectrum estimation

T2 - A method demonstration and new limits from early Murchison Widefield Array 128-tile data EMPIRICAL COVARIANCE MODELING for 21 CM POWER .. JOSHUA S. DILLON et al.

AU - Dillon, Joshua S.

AU - Neben, Abraham R.

AU - Hewitt, Jacqueline N.

AU - Tegmark, Max

AU - Barry, N.

AU - Beardsley, A. P.

AU - Bowman, Judd

AU - Briggs, F.

AU - Carroll, P.

AU - De Oliveira-Costa, A.

AU - Ewall-Wice, A.

AU - Feng, L.

AU - Greenhill, L. J.

AU - Hazelton, B. J.

AU - Hernquist, L.

AU - Hurley-Walker, N.

AU - Jacobs, Daniel

AU - Kim, H. S.

AU - Kittiwisit, P.

AU - Lenc, E.

AU - Line, J.

AU - Loeb, A.

AU - McKinley, B.

AU - Mitchell, D. A.

AU - Morales, M. F.

AU - Offringa, A. R.

AU - Paul, S.

AU - Pindor, B.

AU - Pober, J. C.

AU - Procopio, P.

AU - Riding, J.

AU - Sethi, S.

AU - Shankar, N. Udaya

AU - Subrahmanyan, R.

AU - Sullivan, I.

AU - Thyagarajan, Nithyanandan

AU - Tingay, S. J.

AU - Trott, C.

AU - Wayth, R. B.

AU - Webster, R. L.

AU - Wyithe, S.

AU - Bernardi, G.

AU - Cappallo, R. J.

AU - Deshpande, A. A.

AU - Johnston-Hollitt, M.

AU - Kaplan, D. L.

AU - Lonsdale, C. J.

AU - McWhirter, S. R.

AU - Morgan, E.

AU - Oberoi, D.

AU - Ord, S. M.

AU - Prabu, T.

AU - Srivani, K. S.

AU - Williams, A.

AU - Williams, C. L.

PY - 2015/6/19

Y1 - 2015/6/19

N2 - The separation of the faint cosmological background signal from bright astrophysical foregrounds remains one of the most daunting challenges of mapping the high-redshift intergalactic medium with the redshifted 21 cm line of neutral hydrogen. Advances in mapping and modeling of diffuse and point source foregrounds have improved subtraction accuracy, but no subtraction scheme is perfect. Precisely quantifying the errors and error correlations due to missubtracted foregrounds allows for both the rigorous analysis of the 21 cm power spectrum and for the maximal isolation of the "EoR window" from foreground contamination. We present a method to infer the covariance of foreground residuals from the data itself in contrast to previous attempts at a priori modeling. We demonstrate our method by setting limits on the power spectrum using a 3 h integration from the 128-tile Murchison Widefield Array. Observing between 167 and 198 MHz, we find at 95% confidence a best limit of Δ2(k)

AB - The separation of the faint cosmological background signal from bright astrophysical foregrounds remains one of the most daunting challenges of mapping the high-redshift intergalactic medium with the redshifted 21 cm line of neutral hydrogen. Advances in mapping and modeling of diffuse and point source foregrounds have improved subtraction accuracy, but no subtraction scheme is perfect. Precisely quantifying the errors and error correlations due to missubtracted foregrounds allows for both the rigorous analysis of the 21 cm power spectrum and for the maximal isolation of the "EoR window" from foreground contamination. We present a method to infer the covariance of foreground residuals from the data itself in contrast to previous attempts at a priori modeling. We demonstrate our method by setting limits on the power spectrum using a 3 h integration from the 128-tile Murchison Widefield Array. Observing between 167 and 198 MHz, we find at 95% confidence a best limit of Δ2(k)

UR - http://www.scopus.com/inward/record.url?scp=84936747459&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84936747459&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.91.123011

DO - 10.1103/PhysRevD.91.123011

M3 - Article

AN - SCOPUS:84936747459

VL - 91

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 1550-7998

IS - 12

M1 - 123011

ER -