Molecular gas filamentary structures in galaxy clusters
arXiv:1807.07027 · doi:10.1017/S1743921318003915
Abstract
Recent molecular line observations with ALMA and NOEMA in several Brightest Cluster Galaxies (BCG) have revealed the large-scale filamentary structure at the center of cool core clusters. These filaments extend over 20-100kpc, they are tightly correlated with ionized gas (H, [NII]) emission, and have characteristic shapes: either radial and straight, or also showing a U-turn, like a horse-shoe structure. The kinematics is quite regular and laminar, and the derived infall time is much longer than the free-fall time. The filaments extend up to the radius where the cooling time becomes larger than the infall time. Filaments can be perturbed by the sloshing of the BCG in its cluster, and spectacular cooling wakes have been observed. Filaments tend to occur at the border of cavities driven in the X-ray gas by the AGN radio jets. Observations of cool core clusters support the thermal instability scenario, which accounts for the multiphase medium in the upper atmospheres of BCG, where the right balance between heating and cooling is reached, and a chaotic cold gas accretion occurs. Molecular filaments are also seen associated to ram-pressure stripped spiral galaxies in rich galaxy clusters, and in jet-induced star formation, suggesting a very efficient molecular cloud formation even in hostile cluster environments.
8 pages, 4 figures, in IAU-S342 -- Perseus in Sicily: from black hole to cluster outskirts -- K. Asada, E. de Gouveia dal Pino, H. Nagai, R. Nemmen, M. Giroletti, eds
References in corpus (12)
- Accretion of gas onto nearby spiral galaxies
- Regulation of star formation in giant galaxies by precipitation, feedback, and conduction
- Unifying the micro and macro properties of AGN feeding and feedback
- Abundant molecular gas and inefficient star formation in intracluster regions: Ram pressure stripped tail of the Norma galaxy ESO137-001
- The origin of fast molecular outflows in quasars: molecule formation in AGN-driven galactic winds
- A Spectacular H Complex in Virgo: Evidence for a Collision Between M86 and NGC 4438 and Implications for Collisional ISM Heating of Ellipticals
- The Origin of Molecular Clouds In Central Galaxies
- Molecular Gas in the X-ray Bright Group NGC 5044 as Revealed by ALMA
- ALMA observations of molecular clouds in three group centered elliptical galaxies: NGC 5846, NGC 4636, and NGC 5044
- Close entrainment of massive molecular gas flows by radio bubbles in the central galaxy of Abell 1795
- Filamentary Star Formation in NGC 1275
- On the Formation of Molecular Clumps in QSO Outflows