(a) Median SFR for galaxies in different parts of the cosmic web from the field to clusters for different redshift bins. We clearly see a gradual decline in the median SFR from the field to clusters at z ≲ 0.8 but at higher redshifts (z ≳ 0.8), the trend flattens out. The decline in the median SFR from the field to filaments is not significantly large but the SFR difference between cluster galaxies and those located in other regions of the cosmic web is quite evident at z ≲ 0.8. (b) Median SFR for satellite galaxies located in different regions of the comic web at different redshifts. These trends are very similar to the overall population of galaxies, indicating the dominance of satellites in determining the general trends. At ﹩0.1\leqslant z\leqslant 0.5﹩, the median SFR of satellites decreases by ∼1 dex as one goes from the field to clusters. (c) Median SFR of central galaxies in the comic web at different redshifts. In the whole redshift range considered here, the median SFR of central galaxies decreases by ∼0.5 dex from the field to clusters. (d) Median SFR of isolated galaxies in the comic web at different redshifts. Isolated systems at z ≲ 0.8 show similar trends to centrals, whereas at z ≳ 0.8, their trend resembles that of satellites. (e)–(h) Median stellar mass for all, satellite, central, and isolated galaxies in the cosmic web, respectively. Within the uncertainties, we see almost no change or a slight increase in some cases (∼0.2–0.3 dex in maximum) in the median stellar mass of galaxies from the field to clusters. Therefore, stellar mass differences in different parts of the cosmic web cannot much explain these trends or make them even stronger.