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Fig. 3.


Lyα haloes spectral analysis of the six galaxies presented in Fig. 2. First row: peak velocity shift relative to the central Lyα line () plotted against the FWHM of the Lyα lines extracted in the different Voronoi bins for the six tested objects (MUSE IDs are indicated). The brightness of the points indicates the bin surface brightness (darker point meaning higher SB). Pearson correlation coefficients ρ and corresponding p0 values are shown in each panel. The solid colored line indicates the best fit of our data, while the dashed colored lines show the 1σ errors (the slope α and its error are indicated in the legend). The square point (last panel) is discarded for the fit (sigma clipping factor of 4). The parameters measured on the total Lyα lines are indicated by the star symbols. For comparison the re-scaled V18 relation (solid line) and its dispersion (dotted lines) are plotted in black. The black dashed lines show the V18 relation 1σ errors by taking into account the errors of the re-scaling procedure (see Sect. 3.3.2). Bottom rows: Lyα surface brightness of the bins as a function of the peak velocity shift (top) and FWHM (bottom) of the Lyα line for the six tested objects. The black dotted vertical lines indicate the central Lyα line values. The black horizontal dashed line represents the arbitrary SB threshold at 10−17 erg s−1 cm−2 arcsec−2. The colored vertical dashed lines show the median values of the SB < 10−17 erg s−1 cm−2 arcsec−2 bins.

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