  The intergalactic medium (IGM) accounts for ~90% of baryons at all epochs and
yet its three dimensional distribution in the cosmic web remains mostly
unknown. This is so because the only feasible way to observe the bulk of the
IGM is through intervening absorption line systems in the spectra of bright
background sources, which limits its characterization to being one-dimensional.
Still, an averaged three dimensional picture can be obtained by combining and
cross-matching multiple one-dimensional IGM information with three-dimensional
galaxy surveys. Here, we present our recent and current efforts to map and
characterize the IGM in the cosmic web using galaxies as tracers of the
underlying mass distribution. In particular, we summarize our results on: (i)
IGM around star-forming and non-star-forming galaxies; (ii) IGM within and
around galaxy voids; and (iii) IGM in intercluster filaments. With these
datasets, we can directly test the modern paradigm of structure formation and
evolution of baryonic matter in the Universe.
