Dissecting the Perseus-Pisces supercluster observed with CFHT-MegaCam. Investigating environmental effects on galaxy morphology

Le résumé fourni par la source

The discovery of the large-scale structure of the Universe has fundamentally reshaped our understanding of galaxy formation and evolution. Filaments of the cosmic web act as privileged environments, guiding the growth of structures. Motivated by predictions from cosmological simulations, we investigate the morphological distribution of galaxies within the Perseus-Pisces Supercluster, a prominent nearby filamentary structure at ∼70 Mpc. In particular, we examine how galaxy morphology and structural perturbations correlate with location in the filament network and with proximity to dense nodes. We construct a galaxy sample from a spectroscopic catalogue cross-matched with deep r-band CFHT/MegaCam imaging from the Ultraviolet Near-Infrared Optical Northern Survey, enabling the exploration of low surface brightness features and the detection of extended outer structures. Galaxy morphologies are classified both visually and via structural parameters derived from surface brightness profiles, using the and softwares. The 3D filamentary skeleton of the Perseus-Pisces Supercluster is extracted using the algorithm, allowing the computation of the perpendicular distance of each galaxy to the nearest filament (d_ AutoProf AstroPhot DisPerSE fil ) and to group/cluster centres (d_ gr,cl ). The 3D reconstruction uncovers a network of interconnected sub-filaments converging around the Pisces cluster, forming a complex, multi-branched supercluster-scale structure that likely governs environmental influences on galaxy evolution. We find clear evidence of morphological and stellar mass segregation within the Perseus-Pisces Supercluster: massive early-type galaxies (E/S0) predominantly reside along the spine of filaments and in the vicinity of dense nodes, whereas late-type and irregular systems are more diffusely distributed throughout the network. Approximately 10-13% of galaxies display pronounced signatures of gravitational interaction, with stellar halo asymmetries being most common in filaments and groups. Together, these results highlight the dual role of filamentary environments, both as sites hosting evolved early-type systems and as regions where local tidal interactions and pre-processing significantly affect galaxy morphology.

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