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We explore the radial distribution of satellite galaxies in groups in theGalaxy and Mass Assembly (GAMA) survey and the IllustrisTNG simulations.Considering groups with masses $12.0 \leq \log_{10} (\mathcal{M}_h / h^{-1}\mathrm{M}_{\odot}) < 14.8$ at $z<0.267$, we find a good agreement between GAMAand a sample of TNG300 groups and galaxies designed to match the GAMAselection. Both display a flat profile in the centre of groups, followed by adecline that becomes steeper towards the group edge, and normalised profilesshow no dependence on group mass. Using matched satellites from TNG and darkmatter-only TNG-Dark runs we investigate the effect of baryons on satelliteradial location. At $z=0$, we find that the matched subhaloes from the TNG-Darkruns display a much flatter radial profile: namely, satellites selected above aminimum stellar mass exhibit both smaller halo-centric distances and longersurvival times in the full-physics simulations compared to their dark-matteronly analogues. We then divide the TNG satellites into those which possessTNG-Dark counterparts and those which do not, and develop models for the radialpositions of each. We find the satellites with TNG-Dark counterparts aredisplaced towards the halo centre in the full-physics simulations, and thisdifference has a power-law behaviour with radius. For the `orphan' galaxieswithout TNG-Dark counterparts, we consider the shape of their radialdistribution and provide a model for their motion over time, which can be usedto improve the treatment of satellite galaxies in semi-analytic andsemi-empirical models of galaxy formation.

Exploring the effect of baryons on the radial distribution of satellite galaxies with GAMA and IllustrisTNG