English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The separation of the faint cosmological background signal from brightastrophysical foregrounds remains one of the most daunting challenges ofmapping the high-redshift intergalactic medium with the redshifted 21 cm lineof neutral hydrogen. Advances in mapping and modeling of diffuse and pointsource foregrounds have improved subtraction accuracy, but no subtractionscheme is perfect. Precisely quantifying the errors and error correlations dueto missubtracted foregrounds allows for both the rigorous analysis of the 21 cmpower spectrum and for the maximal isolation of the "EoR window" fromforeground contamination. We present a method to infer the covariance offoreground residuals from the data itself in contrast to previous attempts at apriori modeling. We demonstrate our method by setting limits on the powerspectrum 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 ofDelta^2(k) < 3.7 x 10^4 mK^2 at comoving scale k = 0.18 hMpc^-1 and at z = 6.8,consistent with existing limits.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d, particles, fields, gravitation, and cosmology

Empirical Covariance Modeling for 21 cm Power Spectrum Estimation: A  Method Demonstration and New Limits from Early Murchison Widefield Array  128-Tile Data