Topology of LargeScale Structure in Seeded Hot Dark Matter Models
Abstract
We examine the topology of the isodensity surfaces in seeded hot dark matter models, in which static seed masses provide the density perturbations in a universe dominated by massive neutrinos. When smoothed with a Gaussian window W(r) = e ^r^2^/ro^2^^ the linear initial conditions in these models show no trace of nonGaussian behavior for r_0_ >= 5 Mpc (h = 1/2 ), except for very low seed densities, which show a shift toward isolated peaks. An approximate analytic expression is given for the genus curve expected in linear density fields from randomly distributed seed masses. The evolved models have a Gaussian topology for r_0_ = 10 Mpc, but show a shift toward a cellular topology with r_0_ = 5 Mpc; Gaussian models with an identical power spectrum show the same behavior. Contour plots can distinguish between the seeded hot dark matter model and the Gaussian model with an identical initial power spectrum: after equal evolution in the expansion factor, the seeded hot dark matter model produces more coherent structure; the highdensity regions form a network of connected filaments, while the lowdensity regions in this model are made up of large welldefined voids.
 Publication:

The Astrophysical Journal
 Pub Date:
 March 1992
 DOI:
 10.1086/171097
 Bibcode:
 1992ApJ...387..443B
 Keywords:

 Dark Matter;
 Elementary Particles;
 Galactic Clusters;
 Space Density;
 Astronomical Models;
 Density Distribution;
 Neutrinos;
 Power Spectra;
 Topology;
 Astrophysics;
 COSMOLOGY: DARK MATTER;
 COSMOLOGY: LARGESCALE STRUCTURE OF UNIVERSE;
 ELEMENTARY PARTICLES;
 GALAXIES: CLUSTERING