# Dark Matter Response to Galaxy Assembly History

## TL;DR

This study investigates how galaxy assembly history influences dark matter halo properties over time, revealing that halo profiles stabilize when baryonic mass in the center reaches 80%, with earlier assembly linked to quicker stabilization.

## Contribution

It demonstrates the connection between baryonic assembly history and dark matter halo evolution, emphasizing the importance of stellar mass content in halo contraction models.

## Key findings

- Dark matter halo profiles stabilize when 80% of baryons are centrally accumulated.
- Earlier assembled haloes contain more baryonic mass at earlier times.
- Halo contraction models should incorporate stellar mass content for accuracy.

## Abstract

Aims: It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods: We study the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between $z = 0 - 4$. In this work, we use the SPH run from Scannapieco et al. (2009) and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compare them with one of the haloes run using a moving-mesh technique and different sub-grid scheme. Results: Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 percent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five percent of the virial radius at z = 0, remains approximately constant from the time at which 60 percent of the stellar mass is gathered. We explore different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.