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Fig. A.2.


Flux calibration. Left panel: we fit the baseline from the data shown in green dots with the function A * sin(kx + b)+mx + n to account for the stand wave. Right panel: we correct the Doppler velocity and convert the antenna temperatures to flux intensities in mJy. H I emission from galaxies should have no polarisation. As a consistency check, we also reduce the spectrum including only one polarisation, and show the results in blue and red.

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