Stellar mass and morphology segregation into pairs and multiplets in the cosmic web

In this work, we investigate whether the location of galaxies within the large-scale structures (LSS) of the Universe leaves an imprint on their stellar mass (M_⋆) and morphology. To this end, we attempt to disentangle the effects of local and large-scale environments on these distributions. We classified a sample of 25, 309 galaxies in the redshift range 0. 02 < z łeq 0. 04 with łog M_⋆/ _⊙ ≥ 9. 5 according to both the main LSS environments of voids, clusters, and regions that are neither clusters nor voids (hereafter NCNV) and the local environment (singlets and multiplets; galaxies with and without companions). We present the stellar mass and morphology distributions in these environments, as well as for a subsample of galaxy pairs. M Even in the voids, we find that sim22% of galaxies have companions. The stellar mass distributions show that galaxies are significantly less massive in voids, regardless of their local environment. Satellites in voids are also less massive relative to their centrals than satellites in NCNV pairs. In terms of morphology, the denser the LSS, the greater is the proportion of early-type galaxies, even among singlets. In voids and NCNV regions, late-type multiplets tend to be later-type spirals rather than singlets. In pairs, centrals tend to be earlier-type than satellites. The sample, which we curated to avoid morphology incompleteness, yields slightly higher fractions of early-type galaxies and multiplets than previous studies. We conclude that the local environment alone is not sufficient to explain the distribution of stellar mass and morphology of galaxies in the local Universe. The observed mass distributions are consistent with a scenario in which the assembly of galaxies depends critically on their host halos, and the properties of these halos are related to their large-scale environment. This would explain the presence of lower-mass galaxies in voids than in denser environments and provides a basis for considering a common evolutionary origin for multiplets.