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We found a bug in the procedure we used to calculate the metallicity and ionization parameter that led to an underestimation of these quantities.
While none of the conclusions and trends are affected, the absolute values in Figures 1 and 2 (Figures 11 and 14 in the original paper) change as illustrated in the figures below. Values in the text should be updated accordingly in a few sentences as follows:
Figure 1. Figure 11 in the original paper. Metallicity (left) and ionization parameter (right) map. The central region powered by an AGN according to the Baldwin–Phillips–Terlevich [N ii]6583/Hα diagnostic has been masked (gray area). Contours are stellar isophotes, the same as in Figure 4 in the paper.
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Figure 2. Figure 14 in the original paper. Metallicity (left) and q ionization parameter (right) of the knots. The gray shaded area represents the Hα image.
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In Section 7.3. The metallicity in the tentacles is high to intermediate, reaching lowest values of ∼12 + log[O/H] = 8.5 in the furthest regions of the west tail and throughout the southern tail.
Finally, the right panel of Figure 1 shows that the ionization parameter is overall rather low (typically between log q = 6.7 and 7.5) compared to the distribution measured in SDSS emission-line galaxies of all masses (always >7, typically 7.3;....).
In Section 7.4. The knots south of the disk, on the southern side of the main tail, and those at the highest distances in the tail to the west are the most metal-poor (12 + log(O/H) = 8.5–8.7). The majority of the rest of the knots have higher metallicities (8.8–9.0), while the most metal-rich significant knots are located along the disk northwest of the galaxy center.
In Section 8. The metallicity of the gas varies significantly from some very metal-rich regions in the disk to intermediate metallicities in some of the tails.