CHIPS: The Cosmological H I Power Spectrum Estimator
Journal
Date Issued
2016
Author(s)
Trott, C. M.
•
Pindor, B.
•
Procopio, P.
•
Wayth, R. B.
•
Mitchell, D. A.
•
McKinley, B.
•
Tingay, S. J.
•
Barry, N.
•
Beardsley, A. P.
•
•
Bowman, Judd D.
•
Briggs, F.
•
Cappallo, R. J.
•
Carroll, P.
•
de Oliveira-Costa, A.
•
Dillon, Joshua S.
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Ewall-Wice, A.
•
Feng, L.
•
Greenhill, L. J.
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Hazelton, B. J.
•
Hewitt, J. N.
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Hurley-Walker, N.
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Johnston-Hollitt, M.
•
Jacobs, Daniel C.
•
Kaplan, D. L.
•
Kim, H. S.
•
Lenc, E.
•
Line, J.
•
Loeb, A.
•
Lonsdale, C. J.
•
Morales, M. F.
•
Morgan, E.
•
Neben, A. R.
•
Thyagarajan, Nithyanandan
•
Oberoi, D.
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Offringa, A. R.
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Ord, S. M.
•
Paul, S.
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Pober, J. C.
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Prabu, T.
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Riding, J.
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Udaya Shankar, N.
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Sethi, Shiv K.
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Srivani, K. S.
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Subrahmanyan, R.
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Sullivan, I. S.
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Tegmark, M.
•
Webster, R. L.
•
Williams, A.
•
Williams, C. L.
•
Wu, C.
•
Wyithe, J. S. B.
Abstract
Detection of the cosmological neutral hydrogen signal from the Epoch of Reionization (EoR) and estimation of its basic physical parameters are principal scientific aims of many current low-frequency radio telescopes. Here we describe the Cosmological H I Power Spectrum Estimator (CHIPS), an algorithm developed and implemented with data from the Murchison Widefield Array, to compute the two-dimensional and spherically-averaged power spectrum of brightness temperature fluctuations. The principal motivations for CHIPS are the application of realistic instrumental and foreground models to form the optimal estimator, thereby maximizing the likelihood of unbiased signal estimation, and allowing a full covariant understanding of the outputs. CHIPS employs an inverse-covariance weighting of the data through the maximum likelihood estimator, thereby allowing use of the full parameter space for signal estimation (“foreground suppression”). We describe the motivation for the algorithm, implementation, application to real and simulated data, and early outputs. Upon application to a set of 3 hr of data, we set a 2σ upper limit on the EoR dimensionless power at k=0.05 {{h}} Mpc-1 of {{{∆ }}}k2\lt 7.6× {10}4 mK2 in the redshift range z = [6.2-6.6], consistent with previous estimates.
Volume
818
Issue
2
Start page
139
Issn Identifier
0004-637X
Ads BibCode
2016ApJ...818..139T
Rights
open.access
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