Detecting the H i power spectrum in the post-reionization Universe with SKA-Low - INSPIRE

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Detecting the H i power spectrum in the post-reionization Universe with SKA-Low

Zhaoting Chen
(
- Jodrell Bank and
- U. Manchester (main)
)
,
Emma Chapman
(
- Nottingham U.
)
,
Laura Wolz
(
- Jodrell Bank and
- U. Manchester (main)
)
,
Aishrila Mazumder
(
- Jodrell Bank and
- U. Manchester (main)
)

Feb 22, 2023

17 pages

Published in:

Mon.Not.Roy.Astron.Soc. 524 (2023) 3, 3724-3740,
Mon.Not.Roy.Astron.Soc. 524 (2023) 3, 3724-3740

Published: Jul 24, 2023

e-Print:

2302.11504 [astro-ph.CO]

DOI:

10.1093/mnras/stad2102

View in:

ADS Abstract Service

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Abstract: (Oxford University Press)

We present a survey strategy to detect the neutral hydrogen (H i) power spectrum at 5 < z < 6 using the SKA-Low radio telescope in presence of foregrounds and instrumental effects. We simulate observations of the inherently weak H i signal post-reionization with varying levels of noise and contamination with foreground amplitudes equivalent to residuals after sky model subtraction. We find that blind signal separation methods on imaged data are required in order to recover the H i signal at large cosmological scales. Comparing different methods of foreground cleaning, we find that Gaussian Process Regression (GPR) performs better than Principle Component Analysis (PCA), with the key difference being that GPR uses smooth kernels for the total data covariance. The integration time of one field needs to be larger than ∼250 h to provide large enough signal-to-noise ratio (SNR) to accurately model the data covariance for foreground cleaning. Images within the primary beam field-of-view give measurements of the H i power spectrum at scales |

k\sim 0.02\, {\rm Mpc^{-1}}-0.3\, {\rm Mpc^{-1} }

| with SNR ∼2–5 in Δ[log(k/Mpc^−1)] = 0.25 bins assuming an integration time of 600 h. Systematic effects, which introduce small-scale fluctuations across frequency channels, need to be ≲ 5 × 10^−5 to enable unbiased measurements outside the foreground wedge. Our results provide an important validation towards using the SKA-Low array for measuring the H i power spectrum in the post-reionization Universe.

Note:

17 pages, 22 figures. Updated to match the published version in MNRAS

techniques: interferometric
(cosmology:) large-scale structure of Universe
radio lines: general

References(224)

Figures(23)

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