2025MNRAS.541.3220D

Determining the processes by which galaxies transition from a star-forming to a quiescent state (quenching) is paramount to our understanding of galaxy evolution. One of the key mechanisms by which this takes place is via a galaxy's interactions with a local, overdense environment (satellite or environmental quenching). In the very local Universe, we see these processes in action, and can also observe their effects via the distribution of satellite galaxy properties. However, extending similar analyses outside of the local Universe is problematic, largely due to the difficulties in robustly defining environments with small and/or incomplete spectroscopic samples. We use new environmental metrics from the high-completeness Deep Extragalactic VIsible Legacy Survey (DEVILS) to explore the properties of satellite galaxies at intermediate redshift (0.3$<$z$<$0.5) and compare directly to the Galaxy And Mass Assembly Survey (GAMA) at 0$<$z$<$0.2. Importantly, both the galaxy properties and environmental metrics in DEVILS and GAMA are derived in an identical manner, reducing any methodology biases. We find: (i) that satellite galaxies in DEVILS and GAMA show suppressed star formation in comparison to isolated systems at the same stellar mass, by $\sim$0.5 dex in log$_{10}$(SFR/M$_{\odot }$ yr$^{-1}$), (ii) that this suppression is strongest in higher mass dark matter haloes (up to $\sim$1 dex in log$_{10}$(SFR/M$_{\odot }$ yr$^{-1}$) in the most massive haloes), and (iii) that at fixed stellar and halo mass, this suppression increases with time - with satellite passive fractions increasing by $\sim$10-15 per cent over the last $\sim$5 Gyr. This is consistent with previous observations and numerical simulations.