Secondary infall model and dark matter scaling relations in intermediate redshift early - type galaxies

TL;DR

This paper uses an updated secondary infall model to predict dark matter halo profiles in intermediate redshift early-type galaxies, linking theoretical models with observational data to explore dark matter scaling relations.

Contribution

It introduces a simplified, one-parameter halo profile model that fits observational data and investigates dark matter scaling relations in galaxies.

Findings

The model accurately fits lens galaxy data.

Dark matter column density correlates with stellar and virial mass.

Dark matter acceleration shows specific scaling relations.

Abstract

Scaling relations among dark matter (DM) and stellar quantities are a valuable tool to constrain formation scenarios and the evolution of galactic structures. However, most of the DM properties are actually not directly measured, but derived through model dependent mass mapping procedures. It is therefore crucial to adopt theoretically and observationally well founded models. We use here an updated version of the secondary infall model (SIM) to predict the halo density profile, taking into account the effects of angular momentum, dissipative friction and baryons collapse. The resulting family of halo profiles depends on one parameter only, the virial mass, and nicely fits the projected mass and aperture velocity dispersion of a sample of intermediate redshift lens galaxies. We derive DM related quantities (namely the column density and the Newtonian acceleration) and investigate their correlations with stellar mass, luminosity, effective radius and virial mass.