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Context. Understanding the formation, evolution and present-day
properties of the cosmic web and objects forming it is an important task in cosmology.
Aims. We compare the galaxy populations in superclusters of different
morphology in the nearby Universe (180 h-1 Mpc
≤ d ≤ 270 h-1 Mpc) to see whether the inner
structure and overall morphology of superclusters are important in shaping galaxy
properties in superclusters.
Methods. We find supercluster morphology with Minkowski functionals and
analyse the probability density distributions of colours, morphological types, stellar
masses, star formation rate (SFR) of galaxies, and the peculiar velocities of the main
galaxies in groups in superclusters of filament and spider types, and in the field. We
test the statistical significance of the results with the KS test.
Results. The fraction of red, early-type, low SFR galaxies in
filament-type superclusters is higher than in spider-type superclusters; in low-density
global environments their fraction is lower than in superclusters. In all environments the
fraction of red, high stellar mass, and low SFR galaxies in rich groups is higher than in
poor groups. In superclusters of spider morphology red, high SFR galaxies have higher
stellar masses than in filament-type superclusters. Groups of equal richness host galaxies
with larger stellar masses, a larger fraction of early-type and red galaxies, and a higher
fraction of low SFR galaxies, if they are located in superclusters of filament morphology.
The peculiar velocities of the main galaxies in groups from superclusters of filament
morphology are higher than in those of spider morphology. Groups with higher peculiar
velocities of their main galaxies in filament-type superclusters are located in higher
density environment than those with low peculiar velocities. There are significant
differences between galaxy populations of the individual richest superclusters.
Conclusions. Both local (group) and global (supercluster) environments
and even supercluster morphology play an important role in the formation and evolution of
galaxies. Differences in the inner structure of superclusters of filament and spider
morphology and the dynamical state of galaxy groups in them may lead to the differences
found in our study
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