Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data
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 sou...
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| Format: | Article |
| Language: | English |
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American Physical Society
2015
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| Online Access: | http://hdl.handle.net/1721.1/97502 https://orcid.org/0000-0002-4117-570X https://orcid.org/0000-0001-7776-7240 https://orcid.org/0000-0001-7130-208X https://orcid.org/0000-0002-0086-7363 https://orcid.org/0000-0003-3336-9958 https://orcid.org/0000-0001-7670-7190 https://orcid.org/0000-0003-0422-2324 |
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| author | Barry, N. Beardsley, A. P. Bowman, Judd D. Briggs, Frank H. Carroll, P. Greenhill, Lincoln J. Hazelton, B. J. Hernquist, L. Hurley-Walker, N. Jacobs, Daniel C. Kim, H. S. Kittiwisit, P. Lenc, Emil Line, J. Loeb, Abraham McKinley, B. Mitchell, Daniel A. Morales, Miguel 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, Roger J. Deshpande, Ajay A. Johnston-Hollitt, M. Kaplan, David L. Oberoi, Divya Ord, S. M. Prabu, T. Srivani, K. S. Williams, A. Dillon, Joshua Shane Neben, Abraham Richard Tegmark, Max Erik Ewall-Wice, Aaron Michael Feng, Lu Lonsdale, Colin John McWhirter, Stephen R. Williams, Christopher Leigh de Oliveira Costa, Angelica Morgan, Edward H Hewitt, Jacqueline N |
| author2 | Haystack Observatory |
| author_facet | Haystack Observatory Barry, N. Beardsley, A. P. Bowman, Judd D. Briggs, Frank H. Carroll, P. Greenhill, Lincoln J. Hazelton, B. J. Hernquist, L. Hurley-Walker, N. Jacobs, Daniel C. Kim, H. S. Kittiwisit, P. Lenc, Emil Line, J. Loeb, Abraham McKinley, B. Mitchell, Daniel A. Morales, Miguel 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, Roger J. Deshpande, Ajay A. Johnston-Hollitt, M. Kaplan, David L. Oberoi, Divya Ord, S. M. Prabu, T. Srivani, K. S. Williams, A. Dillon, Joshua Shane Neben, Abraham Richard Tegmark, Max Erik Ewall-Wice, Aaron Michael Feng, Lu Lonsdale, Colin John McWhirter, Stephen R. Williams, Christopher Leigh de Oliveira Costa, Angelica Morgan, Edward H Hewitt, Jacqueline N |
| author_sort | Barry, N. |
| collection | MIT |
| description | 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 Δ[superscript 2](k) < 3.7 × 10[superscript 4] mK[superscript 2] at comoving scale k = 0.18 h Mpc[superscript −1] and at z = 6.8, consistent with existing limits. |
| first_indexed | 2024-09-23T15:10:18Z |
| format | Article |
| id | mit-1721.1/97502 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T15:10:18Z |
| publishDate | 2015 |
| publisher | American Physical Society |
| record_format | dspace |
| spelling | mit-1721.1/975022022-09-29T13:07:57Z Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data Barry, N. Beardsley, A. P. Bowman, Judd D. Briggs, Frank H. Carroll, P. Greenhill, Lincoln J. Hazelton, B. J. Hernquist, L. Hurley-Walker, N. Jacobs, Daniel C. Kim, H. S. Kittiwisit, P. Lenc, Emil Line, J. Loeb, Abraham McKinley, B. Mitchell, Daniel A. Morales, Miguel 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, Roger J. Deshpande, Ajay A. Johnston-Hollitt, M. Kaplan, David L. Oberoi, Divya Ord, S. M. Prabu, T. Srivani, K. S. Williams, A. Dillon, Joshua Shane Neben, Abraham Richard Tegmark, Max Erik Ewall-Wice, Aaron Michael Feng, Lu Lonsdale, Colin John McWhirter, Stephen R. Williams, Christopher Leigh de Oliveira Costa, Angelica Morgan, Edward H Hewitt, Jacqueline N Haystack Observatory Lincoln Laboratory Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Dillon, Joshua Shane Neben, Abraham Richard Hewitt, Jacqueline N. Tegmark, Max Erik de Oliveira-Costa, Angelica Ewall-Wice, Aaron Michael Feng, Lu Lonsdale, Colin John McWhirter, Stephen R. Morgan, Edward H. Williams, Christopher Leigh 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 Δ[superscript 2](k) < 3.7 × 10[superscript 4] mK[superscript 2] at comoving scale k = 0.18 h Mpc[superscript −1] and at z = 6.8, consistent with existing limits. National Science Foundation (U.S.) (Grant AST-0457585) National Science Foundation (U.S.) (Grant AST-0821321) National Science Foundation (U.S.) (Grant AST-1105835) National Science Foundation (U.S.) (Grant AST-1410719) National Science Foundation (U.S.) (Grant AST-1410484) National Science Foundation (U.S.) (Grant AST-1411622) National Science Foundation (U.S.) (Grant AST-1440343) MIT School of Science Marble Astrophysics Fund 2015-06-22T16:28:37Z 2015-06-22T16:28:37Z 2015-06 2015-03 2015-06-19T22:00:16Z Article http://purl.org/eprint/type/JournalArticle 1550-7998 1550-2368 http://hdl.handle.net/1721.1/97502 Dillon, Joshua S., et al. "Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data." Phys. Rev. D 91, 123011 (June 2015). © 2015 American Physical Society https://orcid.org/0000-0002-4117-570X https://orcid.org/0000-0001-7776-7240 https://orcid.org/0000-0001-7130-208X https://orcid.org/0000-0002-0086-7363 https://orcid.org/0000-0003-3336-9958 https://orcid.org/0000-0001-7670-7190 https://orcid.org/0000-0003-0422-2324 en http://dx.doi.org/10.1103/PhysRevD.91.123011 Physical Review D Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. American Physical Society application/pdf American Physical Society American Physical Society |
| spellingShingle | Barry, N. Beardsley, A. P. Bowman, Judd D. Briggs, Frank H. Carroll, P. Greenhill, Lincoln J. Hazelton, B. J. Hernquist, L. Hurley-Walker, N. Jacobs, Daniel C. Kim, H. S. Kittiwisit, P. Lenc, Emil Line, J. Loeb, Abraham McKinley, B. Mitchell, Daniel A. Morales, Miguel 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, Roger J. Deshpande, Ajay A. Johnston-Hollitt, M. Kaplan, David L. Oberoi, Divya Ord, S. M. Prabu, T. Srivani, K. S. Williams, A. Dillon, Joshua Shane Neben, Abraham Richard Tegmark, Max Erik Ewall-Wice, Aaron Michael Feng, Lu Lonsdale, Colin John McWhirter, Stephen R. Williams, Christopher Leigh de Oliveira Costa, Angelica Morgan, Edward H Hewitt, Jacqueline N Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title | Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title_full | Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title_fullStr | Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title_full_unstemmed | Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title_short | Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data |
| title_sort | empirical covariance modeling for 21 cm power spectrum estimation a method demonstration and new limits from early murchison widefield array 128 tile data |
| url | http://hdl.handle.net/1721.1/97502 https://orcid.org/0000-0002-4117-570X https://orcid.org/0000-0001-7776-7240 https://orcid.org/0000-0001-7130-208X https://orcid.org/0000-0002-0086-7363 https://orcid.org/0000-0003-3336-9958 https://orcid.org/0000-0001-7670-7190 https://orcid.org/0000-0003-0422-2324 |
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