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Galaxy clusters are connected at their peripheries to the large scalestructures by cosmic filaments that funnel accreting material. Thesefilamentary structures are studied to investigate both environment-drivengalaxy evolution and structure formation and evolution. In the present work, weprobe in a statistical manner the azimuthal distribution of galaxies aroundclusters as a function of the cluster-centric distance, the cluster richness,and the galaxy activity (star-forming or passive).We perform a harmonicdecomposition in large photometric galaxy catalogue around 6400 SDSS clusterswith masses M >1e14 solar masses, in the redshift range of 0.1< z <0.3. Thesame analysis is performed on the mock galaxy catalogue from the light-cone ofMagneticum hydrodynamical simulation.  We use the multipole analysis to quantify asymmetries in the 2-D galaxydistribution. In the inner cluster regions at R <2 R500, we confirm that thegalaxy distribution traces an ellipsoidal shape, which is more pronounced forrichest clusters. In the clusters' outskirts (R= [2-8]R500), filamentarypatterns are detected in harmonic space with a mean angular scale m_mean=4.2+/-0.1. Massive clusters seem to have a larger number of connected filamentsthan low massive ones. We also find that passive galaxies appear to bettertrace the filamentary structures around clusters, even if the contribution ofSF ones tend to increase with the cluster-centric distance, suggesting agradient of galaxy activity in filaments around clusters.

Probing the azimuthal environment of galaxies around clusters. From cluster core to cosmic filaments