Morphology of the Local Volume

TL;DR

This study analyzes the local galaxy distribution's morphology within 8 Mpc using Minkowski functionals, revealing how galaxy clustering and voids vary with luminosity and comparing observations with LambdaCDM simulations.

Contribution

It provides a detailed morphological analysis of the local galaxy distribution and compares observational data with simulated models, highlighting differences in clustering and void emptiness.

Findings

Observed galaxy clustering is stronger than in simulations.

Void regions in real data are emptier than in models.

Morphological features vary with galaxy luminosity.

Abstract

To study the global morphology of the galaxy distribution in our local neighbourhood we calculate the Minkowski functionals for a sequence of volume limited samples within a sphere of 8 Mpc centred on our galaxy. The well known strong clustering of the galaxies and the dominance of voids and coherent structures on larger scales is clearly visible in the Minkowski functionals. The morphology of the galaxy distribution changes with the limiting absolute magnitude. The samples, encompassing the more luminous galaxies, show emptier voids and more pronounced coherent structures. Indeed there is a prominent peak in the luminosity function of isolated galaxies for MB approx. -14, which at least partly explains these morphological changes. We compare with halo samples from a LambdaCDM simulation. Special care was taken to reproduce the observed local neighbourhood as well as the observed luminosity function in these mock samples. All in all the mock samples render the global morphology of the galaxy distribution quite well. However the detailed morphological analysis reveals that real galaxies cluster stronger, the observed voids are emptier and the structures are more pronounced compared to the mock samples from the LambdaCDM simulation.