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Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster
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Author
Russell, H. R.McDonald, M.
McNamara, B. R.
Fabian, A. C.
Nulsen, P. E. J.
Bayliss, M.
Benson, B. A.
Brodwin, Mark
Carlstrom, J. E.
Edge, A. C.
Hlavacek-Larrondo, J.
Marrone, Daniel P.
Reichardt, C. L.
Vieira, J. D.
Affiliation
Univ Arizona, Steward ObservIssue Date
2017-02-14
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IOP PUBLISHING LTDCitation
Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster 2017, 836 (1):130 The Astrophysical JournalJournal
The Astrophysical JournalRights
© 2017. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We report new ALMA observations of the CO(3-2) line emission from the 2.1 +/- 0.3*10(10)M(circle dot). molecular gas reservoir in the central galaxy of the Phoenix cluster. The cold molecular gas is fueling a vigorous starburst at a rate of 500-800M(circle dot)yr(-1) and powerful black hole activity in the forms of both intense quasar radiation and radio jets. The radio jets have inflated huge bubbles filled with relativistic plasma into the hot, X-ray atmospheres surrounding the host galaxy. The ALMA observations show that extended filaments of molecular gas, each 10-20 kpc long with a mass of several billion solar masses, are located along the peripheries of the radio bubbles. The smooth velocity gradients and narrow line widths along each filament reveal massive, ordered molecular gas flows around each bubble, which are inconsistent with gravitational free-fall. The molecular clouds have been lifted directly by the radio bubbles, or formed via thermal instabilities induced in low-entropy gas lifted in the updraft of the bubbles. These new data provide compelling evidence for close coupling between the radio bubbles and the cold gas, which is essential to explain the self-regulation of feedback. The very feedback mechanism that heats hot atmospheres and suppresses star formation may also paradoxically stimulate production of the cold gas required to sustain feedback in massive galaxies.ISSN
1538-4357Version
Final published versionSponsors
ERC [340442]; Natural Sciences and Engineering Council of Canada; Canadian Space Agency Space Science Enhancement Program; NASA [NAS8-03060, HST-GO-13456, GO4-15122A]; Fermi Research Alliance, LLC [De-AC02-07CH11359]; STFC [ST/L00075X/1]; Canada Research Chairs program; Fonds de recherche Nature et technologies; Australian Research Council's Discovery [DP150103208]; United States Department of EnergyAdditional Links
http://stacks.iop.org/0004-637X/836/i=1/a=130?key=crossref.9b607efeb18bd269b55e1442960aedc1ae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/836/1/130