First upper limits on the 21 cm signal power spectrum from cosmic dawn from one night of observations with NenuFAR

Open Access

This article has an erratum: [https://doi.org/10.1051/0004-6361/202450465e]

Table 3.

Imaging parameters used for producing the high-resolution clean images (High Res Clean) and the dirty image cubes for the power spectrum (Dirty Cube).

Parameter	High Res Clean	Dirty Cube
Weighting	Briggs (Robust = −0.1)	Natural
Pixel size	3′	6′
Image size	600 pixels	400 pixels
uv range	> 20λ	5–100λ
Channels	12 (joined)	177 (not joined)
Algorithm	Multiscale (Hogbom)	⋯
Auto mask ^(a)	3	⋯
Auto threshold ^(b)	1	⋯
Mgain ^(c)	0.6	⋯
Spectral pol ^(d)	2 terms	⋯

Notes. The values of parameters not applicable for making dirty images are specified as “⋯”.

^(a)

Threshold at which a mask is constructed from the obtained components.

^(b)

Cleaning threshold based on the local rms.

^(c)

Cleaning gain for major iterations.

^(d)

Number of terms in the polynomial fit over frequency to each clean component.

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