Since their discovery over three decades ago, there has been astounding progress in our understanding of DSFGs. Roughly half all optical and UV emission from star formation is absorbed and re-radiated as infrared light by dust. This dust enshrouded star formation is contained within DSFGs, with some harbouring SFRs of thousands of solar masses per year, yielding infrared luminosities greater than $10^{13}$\,L$_{\odot}$. DSFGs are thought to be the progenitors of elliptical galaxies that are predominantly found within massive, galaxy clusters in the local Universe. This thesis aims to build on this progress by investigating the nature of DSFGs and their environments. We first investigate the molecular gas properties of galaxies in the Antlia cluster, a potentially useful low redshift analogue to developing protoclusters at higher redshifts. We find that the disturbed cluster environment is not strong enough to strip the molecular gas reservoirs of its member galaxies, yielding the observed high SFRs in this population. We also study the properties of candidate members of the massive SpARCS-0330 galaxy cluster at $z \sim 1.6$, where we find significant ongoing star formation. Quenching in SpARCS-0330 is likely driven by secular processes that scale with stellar mass rather than environment, suggesting that either the cluster environment cannot truncate star formation or the galaxy members have not yet inhabited the cluster for long enough to be significantly affected. We also investigate the multiplicities and properties of four candidate z > 4 DSFGs. We find that three resolve into multiple components, suggesting that this population is more diverse than predicted by simulations. We additionally investigate SDSS1607, a fascinating quasar-SMG system at z = 3.65, using observations from the VLA, SMA and HST. Finally, we discuss the implications of these results and the exciting avenues for future research produced by this work.