The ΛCDM cosmological framework provides the standard theoretical description of the large-scale structure of the Universe. Cosmological simulations based on this paradigm predict an intricate network of filaments, clusters, and nodes, collectively known as the cosmic web. Despite these theoretical advances, observational confirmation of this picture remains challenging, particularly in detecting and characterising the diffuse intergalactic medium within cosmic filaments. In this talk, I will review recent progress in the field, focusing on observational strategies that enable identify suitable systems to trace the diffuse gas inside cosmic filaments. I will discuss how insights from cosmological simulations have motivated the development of improved search techniques. 

In particular, I will present our recent work on an enhanced search algorithm that has enabled the systematic identification of promising interacting systems from galaxy redshift surveys. Our results indicate that cluster interactions predominantly taking plance along dense cosmic filaments, with the most energetic interactions concentrated at their prominant nodes. The multi-wavelength properties of these systems provide further insights into the physical processes associated with large-scale structure evolution. Finally, I will discuss the prospects for probing the diffuse, magnetised cosmic web with next-generation radio facilities, such as Square Kilometre Array.