The non-Gaussian distribution of galaxies gravitational fields

TL;DR

This paper presents a theoretical analysis showing that the distribution of galaxy gravitational fields due to tidal interactions is inherently non-Gaussian, influencing galaxy angular momentum alignment and evolution.

Contribution

It introduces a non-Gaussian distribution function for galaxy gravitational fields based on tidal interactions, extending previous models and predicting angular momentum evolution.

Findings

Distribution function is non-Gaussian for tidal interactions

Galaxy angular momentum increases over time

Alignment depends on cluster richness and morphology

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.