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Table 2.

Statistics of fluxes and deconvolved emission, from Gaussian fitting of the clean images of each day.

Deconvolved component (Stokes I) Flux (Stokes I) Flux (Stokes V)



Date Major axis Minor axis PA Peak Integrated Peak Integrated
(dd-mm-yy) (mas) (mas) (deg) (μJy beam−1) (μJy) (μJy beam−1) (μJy)
05-03-22 192 ± 26 60 ± 6 156 ± 6 177 ± 3 216.3 ± 7.7 29.2 ± 2.1 25.4 ± 4.0
09-03-22 118 ± 33 82 ± 15 176 ± 36 146 ± 4 181.4 ± 7.9 < 8.7
10-03-22a 174 ± 33 80 ± 14 178 ± 27 147 ± 3 172.1 ± 6.9 < 9.6
10-03-22b 189 ± 28 85 ± 3 164 ± 8 135 ± 2 158.3 ± 5.1 < 9.6
26-03-22 151 ± 40 99 ± 9 21 ± 8 114 ± 4 173.4 ± 9.0 19.9 ± 2.9 37.4 ± 8.2
27-03-22 231 ± 37 78 ± 16 164 ± 4 88 ± 3 128.1 ± 7.8 < 9.6
30-03-22 255 ± 100 101 ± 34 155 ± 9 75 ± 5 108.0 ± 11.0 < 13.5
31-03-22 192 ± 30 83 ± 11 156 ± 6 101 ± 2 132.7 ± 5.3 < 9.6

All days combined 147 ± 15 69 ± 8 154 ± 7 127 ± 2 157.5 ± 3.5 9.4 ± 0.9 8.1 ± 1.7

Notes. The major and minor axis (FWHM) report the image component size (deconvolved from the beam using gaussfit) and have been taken from the output of CASA task imfit for Stokes I images, along with the value of the position angle. Further, the peak and integrated flux, and the related errors, for both the polarisations have also been calculated by imxfit, by performing a Gaussian fitting. All errors are 1σ, and include only the uncertainty on the fit, and not the overall rms estimated from the images and quoted in Table 1. For the days without significant Stokes V signal, we have provided 3σ upper limits for the peak flux. In the two Stokes V images with a significant detection, gaussfit provided a size of the component (423 ± 126) mas × (150 ± 32) mas for the March 26 observation, while it could not deconvolve the component from the beam for the March 5 observation; hence, a size estimation could not be provided.

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