The non-Gaussian distribution of galaxies gravitational fields

Abstract

We perform a theoretical analysis of the observational dependence between angular momentum of the galaxy clusters and their mass (richness), based on the method introduced in our previous paper. For that we obtain the distribution function of astronomical objects (like galaxies and/or smooth halos of different kinds) gravitational fields due to their tidal interaction. Within the statistical method of Chandrasekhar we are able to show that the distribution function is determined by the form of interaction between objects and for multipole (tidal) interaction it is never Gaussian. Our calculation permits to demonstrate how the alignment of galaxies angular momenta depend on the cluster richness. The specific form of the corresponding dependence is due to assumptions made about cluster morphology. Our approach also predicts the time evolution of stellar objects angular momenta within CDM and $\Lambda$CDM models. Namely, we have shown that angular momentum of galaxies increases with time.

Corrected version. Comparison with observational results and explanations of theoretical method used are added

References in corpus (4)

• The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids
• Angular momentum-Large-scale structure alignments in LCDM models and the SDSS
• The distribution of galaxies gravitational field stemming from their tidal interaction
• Preferred alignments of angular momentum vectors of galaxies in six dynamically unstable Abell clusters

Cited by in corpus (1)

• Investigation of the orientation of galaxies in clusters: the importance, methods and results of research