Observational Signatures of AGN Feedback in the Morphology and the Ionization States of Milky Way-like Galaxies

TL;DR

This study analyzes how different AGN jet models influence galaxy morphology and ionization states, revealing distinct ion distributions and gas pressure effects in Milky Way-like galaxies through simulations.

Contribution

It compares three AGN jet models at different energy levels, highlighting their unique impacts on ion distribution and gas dynamics in galaxy simulations.

Findings

High-energy jets produce isotropic ion distributions with lower densities.

Cosmic ray jets extend cool gas and provide additional pressure support.

A transition in ion-to-mass ratio slope occurs between 10-30 kpc.

Abstract

We make an in-depth analysis of different AGN jet models' signatures, inducing quiescence in galaxies with a halo mass of $10^{12} M_\odot$. Three jet models, including cosmic ray-dominant, hot thermal, and precessing kinetic jets, are studied at two energy flux levels each, compared to a jet-free, stellar feedback-only simulation. We examine the distribution of Mg II, O VI, and O VIII ions, alongside gas temperature and density profiles. Low-energy ions, like Mg II, concentrate in the ISM, while higher energy ions, e.g., O VIII, prevail at the AGN jet cocoon's edge. High-energy flux jets display an isotropic ion distribution with lower overall density. High-energy thermal or cosmic ray jets pressurize at smaller radii, significantly suppressing core density. The cosmic ray jet provides extra pressure support, extending cool and warm gas distribution. A break in the ion-to-mass ratio slope in O VI and O VIII is demonstrated in the ISM-to-CGM transition (between 10-30 kpc), growing smoothly towards the CGM at greater distances.