Abstract
How central galaxies in groups acquired their cold gas is still not fully understood. To unfold this unknown, we map the kinematics and distribution of the optical emission-line gas using MUSE observations of 18 optically selected local brightest group galaxies (BGGs). The observations reveal a distribution of gas morphologies, including complex networks of filaments extending up to ∼10 kpc to compact (<3 kpc) and extended (>5 kpc) disk-dominated structures. By exploring the thermodynamical properties of the X-ray atmospheres, we find most of the filaments and compact have are likely cooled out from the intragroup medium (IGrM).
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