On the largest scales, the Universe contains a network-like distribution of galaxies, gas and dark matter known as the cosmic web. This cosmic web is formed of clusters, walls, voids and filaments, providing a rich environment for galaxies to exist in. Tracing the cosmic web is vital for understanding the evolution of galaxies since several galaxy properties, such as stellar mass, colour, star formation rate (SFR) and specific star formation rate (sSFR) have been shown to be sensitive to the external conditions. In this talk, I will present a way to map the filaments of the cosmic web observationally using galaxies with photometric redshifts. Specifically, I will discuss how we can use the uncertainties in the photometric redshifts to understand how the main components of the cosmic web - the biggest filaments and voids - are still preserved. As well, I will explore how these uncertainties affect the relationships we compute between galaxy properties (stellar mass, specific star formation rate) and the distance to their closest filament.