Violent interaction between the AGN and the hot gas in the core of the galaxy cluster Sersic 159-03

TL;DR

This study investigates the complex interactions between the central AGN, hot gas, and optical nebula in galaxy cluster Sersic 159-03, revealing AGN-driven shocks, gas uplift, and star formation in the cluster core.

Contribution

It provides a multi-wavelength analysis showing how AGN feedback influences the intra-cluster medium and star formation, highlighting new insights into gas dynamics and feedback mechanisms.

Findings

Detection of a high-pressure ring indicating an AGN-driven shock

Identification of a long Halpha+[NII] filament with cooling gas

Evidence of star formation fueled by uplifted, stripped gas

Abstract

We present a multi-wavelength study of the energetic interaction between the central active galactic nucleus (AGN), the intra-cluster medium, and the optical emission line nebula in the galaxy cluster Sersic 159-03. We use X-ray data from Chandra, high resolution X-ray spectra and UV images from XMM-Newton, Halpha images from the SOAR telescope, HST optical imaging, and VLA and GMRT radio data. The cluster center displays signs of powerful AGN feedback, which has cleared the central regions (r<7.5 kpc) of dense, X-ray emitting ICM. X-ray spectral maps reveal a high pressure ring surrounding the central AGN at a radius of r~15 kpc, indicating an AGN driven weak shock. The cluster harbors a bright, 44 kpc long Halpha+[NII] filament extending from the centre of the cD galaxy to the north. Along the filament, we see low entropy, high metallicity, cooling X-ray gas. The gas in the filament has most likely been uplifted by `radio mode' AGN activity and subsequently stripped from the galaxy due to its relative southward motion. Because this X-ray gas has been removed from the direct influence of the AGN jets, part of it cools and forms stars as indicated by the observed dust lanes, molecular and ionized emission line nebulae, and the excess UV emission.