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The wedge bias in reionization 21-cm power spectrum measurements
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy. Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden.;Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden..
Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden.;Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden..
Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden.;Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden..
Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA..
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2016 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 456, no 1, 66-70 p.Article in journal (Refereed) Published
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Abstract [en]

A proposed method for dealing with foreground emission in upcoming 21-cm observations from the epoch of reionization is to limit observations to an uncontaminated window in Fourier space. Foreground emission can be avoided in this way, since it is limited to a wedge-shaped region in k(parallel to), k(perpendicular to) space. However, the power spectrum is anisotropic owing to redshift-space distortions from peculiar velocities. Consequently, the 21-cm power spectrum measured in the foreground avoidance window - which samples only a limited range of angles close to the line-of-sight direction - differs from the full redshift-space spherically averaged power spectrum which requires an average over all angles. In this paper, we calculate the magnitude of this 'wedge bias' for the first time. We find that the bias amplifies the difference between the real-space and redshift-space power spectra. The bias is strongest at high redshifts, where measurements using foreground avoidance will overestimate the redshift-space power spectrum by around 100 per cent, possibly obscuring the distinctive rise and fall signature that is anticipated for the spherically averaged 21-cm power spectrum. In the later stages of reionization, the bias becomes negative, and smaller in magnitude (less than or similar to 20 per cent).

Place, publisher, year, edition, pages
2016. Vol. 456, no 1, 66-70 p.
Keyword [en]
methods: numerical, dark ages, reionization, first stars
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-276785DOI: 10.1093/mnras/stv2679ISI: 000368010000033OAI: oai:DiVA.org:uu-276785DiVA: diva2:903598
Funder
Swedish Research Council, 2012-4144
Available from: 2016-02-16 Created: 2016-02-16 Last updated: 2017-11-30Bibliographically approved

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Jensen, Hannes

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