Gas condensation in brightest group galaxies unveiled with MUSE

The origin of the cold gas in central galaxies groups is still a matter debate. We present Multi-Unit Spectroscopic Explorer (MUSE) observations 18 optically selected local ( z ? 0.017) brightest group (BGGs) to study kinematics and distribution optical emission-line gas. MUSE reveal morphologies including ten complex networks filaments extending up ?10 kpc two compact (< 3 kpc) five extended (> 5 disk-dominated structures. Some rotating disks show rings elongated structures arising from disk. stellar component mainly rotation-dominated, which very different disturbed found filamentary sources. ionized kinematically decoupled for most systems, suggesting an external also find that H ? luminosity correlates with molecular mass. By exploring thermodynamical properties X-ray atmospheres, we are systems small entropy values, K , t cool / eddy ratios. This suggests that, similar cluster (BCGs) core clusters, associated them likely formed hot halo condensations via thermal instabilities, consistent chaotic accretion simulations (as shown C ratio, Ta k plot). note presence gaseous more frequent than BCGs. An explanation those objects contribution fueling by wet mergers or satellites, as qualitatively hinted at some sources sample. Nonetheless, discuss possibility could be transition stage evolutionary sequence filaments, disks, described condensation models cooling flows.