Molecular gas in cool-core brightest cluster galaxies at $z\simeq 0.4$

Abstract

Brightest cluster galaxies (BCG) are today passive and very massive galaxies at the center of their clusters, still accreting mass through swallowing companions, and flows of cold gas, regulated by radio-mode active galactic nucleus (AGN) feedback. However, their formation history is still a matter of debate. We report new results based on millimeter observations performed with the Northern Extended Millimeter Array (NOEMA) interferometer, mapping the cold molecular gas (CO) that feeds the star formation of distant BCGs. We selected three among the strongest cool-core BCGs at intermediate redshifts ($z\simeq 0.4$), namely RX 1532, MACS 1447, and CHIPS 1911. Previous unresolved millimeter observations and multi-wavelength analysis showed that they are among the most star forming ($\mathrm{SFR}\simeq 100M_{\odot }/\mathrm{yr}$) and gas rich ($M_{H_2}\simeq 10^{11}{M}_{\odot }$) BCGs at intermediate redshifts. The selected BCGs are thus caught in a phase of rapid mass assembly, which makes them ideal targets for high-resolution observations of their molecular gas. By combining NOEMA intensity and velocity maps with archival images from the Hubble Space Telescope, we detect in-situ star formation, filaments of accreting cold gas likely regulated by AGN feedback, disturbed morphology associated with tidal tails of molecular gas, as well as gas compression and tails originated from stripping of gas. While effective condensation of the intra-cluster medium is required to explain the large molecular gas reservoirs, the BCGs exhibit a broad variety of environment-driven mechanisms responsible for the processing of their cold gas: flows of cooling gas (RX 1532), ram pressure or sloshing of the intra-cluster medium (MACS 1447), and galactic tides (CHIPS 1911). This study thus sheds new insights on the physical mechanisms responsible for the mass assembly of galaxies hosting AGN at the center of clusters.

18 pages, 10 figures, 4 tables, accepted for publication in Astronomy & Astrophysics, revised version after proofs corrections

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