English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We present new ALMA observations of the molecular gas and far-infraredcontinuum around the brightest cluster galaxy (BCG) in the cool-core clusterMACS 1931.8-2635. Our observations reveal $1.9 \pm 0.3 \times 10^{10}$M$_{\odot}$ of molecular gas, on par with the largest known reservoirs of coldgas in a cluster core. We detect CO(1-0), CO(3-2), and CO(4-3) emission fromboth diffuse and compact molecular gas components that extend from the BCGcenter out to $\sim30$ kpc to the northwest, tracing the UV knots and H$\alpha$filaments observed by HST. Due to the lack of morphological symmetry, wehypothesize that the $\sim300$ km s$^{-1}$ velocity of the CO in the tail isnot due to concurrent uplift by AGN jets, rather we may be observing theaftermath of a recent AGN outburst. The CO spectral line energy distributionsuggests that molecular gas excitation is influenced by processes related toboth star formation and recent AGN feedback. Continuum emission in Bands 6 and7 arises from dust and is spatially coincident with young stars and nebularemission observed in the UV and optical. We constrain the temperature ofseveral dust clumps to be $\lesssim 10$ K, which is too cold to be directlyinteracting with the surrounding $\sim 4.8$ keV intracluster medium (ICM). Thecold dust population extends beyond the observed CO emission and must either beprotected from interacting with the ICM or be surrounded by local volumes ofICM that are several keV colder than observed by Chandra.

The Dust and Molecular Gas in the Brightest Cluster Galaxy in MACS 1931.8-2635