The influence of the Cosmic Web on the properties of dwarf galaxies in the Fornax-Eridanus Supercluster

Abstract

We analyze a sample of low surface brightness dwarf galaxies (mu_e,g > 24.2 mag arcsec^-2), detected using interpretable machine learning tools from the DES survey. We use the Tanoglidis et al. (2021) sample, identified with machine learning, supplemented by Thuruthipilly et al. (2024). We focus on the Fornax-Eridanus Supercluster, where our group determined its 3D filamentary spine using massive galaxies. We study the effect of the large-scale environment on dwarfs in the Fornax-Eridanus Complex. To do this, we compare the properties of dwarfs in clusters, groups, and the field, and examine how these properties vary with distance to the spine of the Fornax Wall. We check if dwarfs trace the Fornax Wall spine, defined by massive galaxies. We identify Fornax Wall members from our photometric dwarf catalog, dividing them into i) within one virial radius of a galaxy group or cluster and ii) outside this radius (field galaxies). We assume dwarfs near the Fornax Wall are at the same distance as the massive galaxies. We then study their distribution within the complex. We probe the morphology-density relation and examine galaxy properties versus distance from the Fornax Wall spine. Red dwarfs are mostly in or near groups close to the Fornax Wall, dominating the population, while blue dwarfs dominate the field. Larger-sized red dwarfs tend to reside in group environments, with significantly larger effective radii than those in the field. Red dwarfs are more concentrated towards the Fornax Wall than blue dwarfs. This suggests that the group environment plays a significant role in the evolution of dwarfs. Mass density distribution in field and group/cluster is similar, indicating the group/cluster population could be an aged version of the field. The group/cluster objects with excess sizes must have been made through interactions in the groups/clusters.

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