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tokens: that BSF galaxies both in the cocoon and in the supercluster have significantly lower stellar masses than galaxies from other populations. This is what could be expected from galaxies which are still forming their stellar content and increasing their stellar mass. Small differences in stellar masses of galaxies from other populations are not statistically significant and we can conclude that galaxies from these populations in our sample have statistically similar stellar masses, in a range of M * ≈ 3 × 10 9 h −1 M ⊙ − 3 × 10 11 h −1 M ⊙ . Figure 10 (upper left panel) shows that BSF galaxies have the highest values of the concentration index, C , and VO galaxies have the lowest C values among our galaxy populations, and they are similar in the supercluster and in the cocoon. In this respect, RQ galaxies differ from others. In the supercluster they have lower values of C than in the cocoon, these differences are statistically significant at a very high level, with a p -value of p ≤ 0.01 (Table 4 ). The distribution of probabilities for galaxies to be of late-type, P late , are plotted in Fig. 10 (upper right panel). This probability is the highest for BSF galaxies and for RQ galaxies in the cocoon, and the lowest for VO galaxies (in both environments). However, KS test shows that these differences are not statistically significant (Table 4 ). BSF galaxies also have the lowest values of stellar velocity dispersions and VO galaxies have the highest (Fig. 10 , lower left panel). This agrees with earlier results which have shown that galaxies with young stellar populations have lower stellar velocity dispersions than galaxies with old stellar populations ( Shankar et al. 2009 ; Bezanson et al. 2012 ; Einasto et al. 2018b ). The stellar velocity dispersions of RQ galaxies are similar in the supercluster and in the cocoon, indicating, in accordance with the results for P late , that the overall morphological type of RQ and RSF galaxies is the same in both environments. As the stellar mass distribution for VO, RQ, and RSF samples are similar, this suggests that VO galaxies are mainly non-rotating early-type galaxies, but RQ and RSF galaxies (and BSF galaxies) may have also a significant rotation component corresponding to the dynamics of disky galaxies. The metallicities Z of BSF, RQ, and RSF galaxies (Fig. 10 , lower right panel) are statistically similar in both environments, BSF and RQ galaxies having the lowest metallicity values. VO galaxies in the supercluster have higher metallicities than galaxies from other populations in our study. In the cocoon, they are similar to the metallicities for galaxies from other populations. We additionally checked whether the galaxy content of long filaments with length ≥20 h −1 Mpc depends on the distance of filament member galaxies from the supercluster centre, D c . The values of D n (4000) index versus D c for galaxies in long filaments are plotted in Fig. 11 . In this figure, background colours show the