Discovery of a diffuse optical line emitting halo in the core of the Centaurus cluster of galaxies: Line emission outside the protection of the filaments

TL;DR

This paper reports the discovery of faint, diffuse optical line emission structures in the Centaurus cluster, extending beyond known filaments, indicating complex gas dynamics and excitation mechanisms in the cluster core.

Contribution

The study presents the first detection of a diffuse optical halo in the Centaurus cluster using MUSE, revealing structures beyond the filaments with distinct kinematic and physical properties.

Findings

Detection of faint diffuse emission structures beyond filaments

Structures are kinematically distinct from the central galaxy

Evidence suggests shocks or pressure imbalances influence gas distribution

Abstract

We present the discovery of diffuse optical line emission in the Centaurus cluster seen with the MUSE IFU. The unparalleled sensitivity of MUSE allows us to detect the faint emission from these structures which extend well beyond the bounds of the previously known filaments. Diffuse structures (emission surrounding the filaments, a northern shell and an extended Halo) are detected in many lines typical of the nebulae in cluster cores ([NII]$_{\lambda 6548\&6583}$ ,[SII]$_{\lambda 6716\&6731}$, [OI]$_{\lambda 6300}$, [OIII]$_{\lambda 4959\&5007}$ etc.) but are more than an order of magnitude fainter than the filaments, with the faint halo only detected through the brightest line in the spectrum ([NII]$_{\lambda 6583}$). These structures are shown to be kinematically distinct from the stars in the central galaxy and have different physical and excitation states to the filaments. Possible origins are discussed for each structure in turn and we conclude that shocks and/or pressure imbalances are resulting in gas dispersed throughout the cluster core, formed from either disrupted filaments or direct cooling, which is not confined to the bright filaments.