Topology of Large - Scale Structure by Galaxy Type : Hydrodynamic Simulations

The topology of large scale structure is studied as a function of galaxy type using the genus statistic. In hydrodynamical cosmological CDM simulations, galaxies form on caustic surfaces (Zeldovich pancakes) then slowly drain onto laments and clusters. The earliest forming galaxies in the simulations (de ned as \ellipticals") are thus seen at the present epoch preferentially in clusters (tending toward a meatball topology), while the latest forming galaxies (de ned as \spirals") are seen currently in a spongelike topology. The topology is measured by the genus (= number of \donut" holes number of isolated regions) of the smoothed density-contour surfaces. The measured genus curve for all galaxies as a function of density obeys approximately the theoretical curve expected for random-phase initial conditions, but the early forming elliptical galaxies show a shift toward a meatball topology relative to the late forming spirals. Simulations using standard biasing schemes fail to show such an e ect. Large observational samples separated by galaxy type could be used to test for this e ect. Cosmology: large-scale structure of Universe { galaxies: clustering { galaxies: formation { hydrodynamics { stars: formation