Environment and mass dependencies of galactic $\lambda$ spin parameter: cosmological simulations and observed galaxies compared

TL;DR

This study compares cosmological simulations and observed galaxies to analyze how the galactic spin parameter $\

Contribution

It introduces a simple model to estimate the spin parameter from observable galaxy properties and compares its distribution across different environments and masses.

Findings

No significant dependence of $\

Low-mass galaxies have higher mean $\

Results constrain galaxy formation mechanisms and angular momentum acquisition.

Abstract

We use a sample of galaxies from the Sloan Digital Sky Survey (SDSS) to search for correlations between the $\lambda$ spin parameter and the environment and mass of galaxies. In order to calculate the total value of $\lambda$ for each observed galaxy, we employed a simple model of the dynamical structure of the galaxies, which allows a rough estimate of the value of $\lambda$ using only readily obtainable observables from the luminous galaxies. Use of a large volume-limited sample (upwards of 11,000) allows reliable inferences of mean values and dispersions of $\lambda$ distributions. We find, in agreement with some N-body cosmological simulations, no significant dependence of $\lambda$ on the environmental density of the galaxies. For the case of mass, our results show a marked correlation with $\lambda$, in the sense that low-mass galaxies present both higher mean values of $\lambda$ and associated dispersions, than high-mass galaxies. These results provide interesting constrain on the mechanisms of galaxy formation and acquisition of angular momentum, a valuable test for cosmological models.