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Title: A 10{sup 10} solar mass flow of molecular gas in the A1835 brightest cluster galaxy

We report ALMA Early Science observations of the A1835 brightest cluster galaxy (BCG) in the CO (3-2) and CO (1-0) emission lines. We detect 5 × 10{sup 10} M {sub ☉} of molecular gas within 10 kpc of the BCG. Its ensemble velocity profile width of ∼130 km s{sup –1} FWHM is too narrow for the molecular clouds to be supported in the galaxy by dynamic pressure. The gas may instead be supported in a rotating, turbulent disk oriented nearly face-on. Roughly 10{sup 10} M {sub ☉} of molecular gas is projected 3-10 kpc to the northwest and to the east of the nucleus with line-of-sight velocities lying between –250 km s{sup –1} and +480 km s{sup –1} with respect to the systemic velocity. The high-velocity gas may be either inflowing or outflowing. However, the absence of high-velocity gas toward the nucleus that would be expected in a steady inflow, and its bipolar distribution on either side of the nucleus, are more naturally explained as outflow. Star formation and radiation from the active galactic nucleus (AGN) are both incapable of driving an outflow of this magnitude. The location of the high-velocity gas projected behind buoyantly rising X-ray cavities and favorablemore » energetics suggest an outflow driven by the radio AGN. If so, the molecular outflow may be associated with a hot outflow on larger scales reported by Kirkpatrick and colleagues. The molecular gas flow rate of approximately 200 M {sub ☉} yr{sup –1} is comparable to the star formation rate of 100-180 M {sub ☉} yr{sup –1} in the central disk. How radio bubbles would lift dense molecular gas in their updrafts, how much gas will be lost to the BCG, and how much will return to fuel future star formation and AGN activity are poorly understood. Our results imply that radio-mechanical (radio-mode) feedback not only heats hot atmospheres surrounding elliptical galaxies and BCGs, but it is able to sweep higher density molecular gas away from their centers.« less
Authors:
; ; ; ;  [1] ;  [2] ;  [3] ; ;  [4] ; ;  [5] ;  [6] ; ;  [7] ;  [8] ; ;  [9] ;  [10] ;  [11] ;  [12]
  1. Department of Physics and Astronomy, University of Waterloo, Waterloo (Canada)
  2. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)
  3. Department of Physics, Durham University, Durham DH1 3LE (United Kingdom)
  4. Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, M5S 3H8 ON (Canada)
  5. L'Observatoire de Paris, 61 Av. de L'Observatoire, F-75014 Paris (France)
  6. Institute of Astronomy, Madingley Road, Cambridge CB3 0HA (United Kingdom)
  7. School of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623 (United States)
  8. Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States)
  9. Department of Physics and Astronomy, Michigan State University, 567 Wilson Road, East Lansing, MI 48824 (United States)
  10. Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721 (United States)
  11. Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo (Netherlands)
  12. European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching (Germany)
Publication Date:
OSTI Identifier:
22357157
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 785; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; ATMOSPHERES; CARBON MONOXIDE; DISTRIBUTION; EMISSION; FEEDBACK; GALAXIES; GALAXY CLUSTERS; GAS FLOW; HEAT; MASS; MOLECULES; STARS; VELOCITY; X RADIATION