Violent interaction between the active galactic nucleus and the hot gas in the core of the galaxy cluster Sérsic 159−03

Abstract

We present a multiwavelength study of the energetic interaction between the central active galactic nucleus (AGN), the intracluster medium (ICM) and the optical emission‐line nebula in the galaxy cluster Sérsic 159−03. We use X‐ray data from Chandra, high‐resolution X‐ray spectra and ultraviolet (UV) images from XMM–Newton, Hα images from the Southern Astrophysics Research Telescope, Hubble Space Telescope optical imaging, and Very Large Array and Giant Metrewave Radio Telescope radio data. The cluster centre displays signs of powerful AGN feedback, which has cleared the central regions (r < 7.5 kpc) of a 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 harbours a bright, 44 kpc long Hα+[N ii] 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.

Feedback in the Cores of Clusters A3581, 2a 0335+096, and Sersic 159-03

“…A curved filament extends north of the BCG nucleus to a radius of ∼35 kpc and comprises a number of filaments and clouds. Hubble Space Telescope observations of the galaxy revealed two lanes of dust absorption that are associated with the emission-line structures (Werner et al 2011). Faint ultraviolet emission is also extended along the filament.…”

“…Emission at 300 MHz is detected at radii of over an arcminute (Bîrzan et al 2008). The radio source has a very steep power-law spectrum (α ∼ −2.2) in the extended emission to the east, northeast, and northwest of the core, and is more shallow in the nucleus (α ∼ −1 to −1.5; Bîrzan et al 2004;Werner et al 2011). The most recent radio output (assumed to be the high-frequency emission) is extended to a radius of ∼10 kpc in each lobe.…”

“…Two inner lobes of radio emission are seen at 5 GHz and 8.5 GHz (Bîrzan et al 2008;Werner et al 2011). The 5 GHz emission is centrally concentrated and the relatively faint lobes are irregular and asymmetric.…”

“…Previous imaging (Hansen et al 2000;Jaffe et al 2005;Crawford & Fabian 1992;McDonald et al 2010;Oonk et al 2010;McDonald et al 2010McDonald et al , 2011Werner et al 2011) in the optical and near-infrared shows several bright filaments surrounding the BCG. A curved filament extends north of the BCG nucleus to a radius of ∼35 kpc and comprises a number of filaments and clouds.…”

“…The core of the cluster has a complex structure at all wavelengths and shows signs of strong AGN feedback (Werner et al 2011;Bîrzan et al 2008).…”