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A complete understanding of the mass assembly history of structures in theuniverse requires the study of the growth of galaxies and their supermassiveblack holes (SMBHs) as a function of their local environment over cosmic time.In this context, it is important to quantify the effects that the early stagesof galaxy cluster development have on the growth of SMBHs. We used a sample ofHerschel/SPIRE sources of $\sim$ 228 red and compact Planck-selectedprotocluster (PC) candidates to estimate the active galactic nuclei (AGN)fraction from a large sample of galaxies within these candidates. We estimatethe AGN fraction by using the mid-infrared (mid-IR) photometry provided by theWISE/AllWISE data of $\sim650$ counterparts at high redshifts. We created anAllWISE mid-IR colour-colour selection using a clustering machine learningalgorithm and two {\it WISE} colour cuts using the 3.4 $\mu m$ (W1), 4.6 $\mum$ (W2) and 12 $\mu m$ (W3) passbands, to classify sources as AGN. We alsocompare the AGN fraction in PCs with that in the field to better understand theinfluence of the environment on galaxy development. We found an AGN fraction of$f_{AGN} = 0.113 \pm 0.03$ in PC candidates and an AGN fraction of $f_{AGN} =0.095 \pm 0.013$ in the field. We also selected a subsample of `red' SPIREsubsample with a higher overdensity significance, obtaining $f_{AGN} = 0.186\pm 0.044$, versus $f_{AGN} = 0.037 \pm 0.010$ of `non-red sources', consistentwith higher AGN fractions for denser environments. We conclude that our resultspoint towards a higher AGN fraction in PCs, similar to other studies.

The AGN fraction in high-redshift protocluster candidates selected by Planck and Herschel