Already early studies of the morphology-density relation of galaxies showed that early-type galaxies lie in the centres of rich clusters, and in small groups in filaments between clusters, where they are located closer to filament axis than late-type galaxies. This means that galaxies are indeed pre-processed in groups. In our present study we searched for quenched galaxies (similar to galaxies in the centres of rich clusters, with the high values of the Dn(4000) parameter) in other environments using SDSS data. We defined global environment using luminosity-density field, and local environment as group membership, where we analysed separately the properties of the brightest group galaxies and satellites. Our study showed that in the lowest global density environment most galaxies are either single or members of very poor groups. Still, approximately 1/3 of all galaxies there are quenched, with very old stellar populations. The distribution of the stellar masses and other properties of single galaxies in all environments are very similar to those of satellite galaxies in high-luminosity clusters. The largest differences are between the brightest group galaxies and satellites, for both high- and low-luminosity groups. Our study shows that, indeed, quenching occurs in groups and among single galaxies both in cluster regions of influence, and far from clusters, in the low-density environments. References: ME 1991 (https://ui.adsabs.harvard.edu/abs/1991MNRAS.252..261E/abstract, https://ui.adsabs.harvard.edu/abs/1991MNRAS.250..802E/abstract) Einasto et al. 2020 (A&A 641, A172, https://ui.adsabs.harvard.edu/abs/2020A%26A...641A.172E/abstract), 2021 (A&A, 649, A51, https://ui.adsabs.harvard.edu/abs/2021A%26A...649A..51E/abstract), 2022 (A&A, 668, A69, (https://ui.adsabs.harvard.edu/abs/2022A%26A...668A..69E/abstract)