One of the best ways to shed light on the possible links between high redshift proto-clusters and galaxy populations is to investigate the clustering properties of these latter ones as they provide a powerful method to constrain halo masses. In this talk I will present clustering results for galaxies with highly enhanced star-formation activity (SFR>30 Msun/yr) and will show that, at redshifts z>~1.5, irrespective of the selection technique and only very mildly depending on their SFR, they all reside in structures of masses > 10^13.5 Msun, i.e. they are ubiquitously located in over-dense structures such as proto-clusters. A striking example of the above result is provided by the distribution of high-redshift star-forming galaxies in the GOODS-South as more than half of these sources is found to reside in an unvirialised, filamentary structure, centered at z~2.2, which extends all along the field. Our data indicate an enhanced star-forming activity for the galaxies belonging to the proto-cluster with respect to those in the field. Finally, we will also show how such structures are a rather common event in the epoch which coincides with the peak of star formation activity.

{"references": ["Magliocchetti M. et al. 2011, MNRAS, 416, 1105", "Magliocchetti M. et al., 2013, MNRAS, 433,127", "Magliocchetti M., Lapi A., Negrello M., De Zotti G., Danese L., 2014, MNRAS, 437, 2263"]}