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We report ALMA Early Science observations of the Abell 1835 brightest clustergalaxy (BCG) in the CO (3-2) and CO (1-0) emission lines. We detect $5\times10^{10}~\rm M_\odot$ of molecular gas within 10 kpc of the BCG. Its ensemblevelocity profile width of $\sim 130 ~\rm km~s^{-1}$ FWHM is too narrow for themolecular cloud sto be supported in the galaxy by dynamic pressure. The gas mayinstead be supported in a rotating, turbulent disk oriented nearly face-on.Roughly $10^{10}~\rm M_\odot$ of molecular gas is projected $3-10 ~\rm kpc$ tothe north-west and to the east of the nucleus with line of sight velocitieslying between $-250 ~\rm km~s^{-1}$ to $+480 ~\rm km~s^{-1}$ with respect tothe systemic velocity. The high velocity gas may be either inflowing oroutflowing. However, the absence of high velocity gas toward the nucleus thatwould be expected in a steady inflow, and its bipolar distribution on eitherside of the nucleus, are more naturally explained as outflow. Star formationand radiation from the AGN are both incapable of driving an outflow of thismagnitude. If so, the molecular outflow may be associated a hot outflow onlarger scales reported by Kirkpatrick and colleagues. The molecular gas flowrate of approximately $200~\rm M_\odot ~yr^{-1}$ is comparable to the starformation rate of $100-180~\rm M_\odot ~yr^{-1}$ in the central disk. How radiobubbles would lift dense molecular gas in their updrafts, how much gas will belost to the BCG, and how much will return to fuel future star formation and AGNactivity are poorly understood. Our results imply that radio-mechanical (radiomode) feedback not only heats hot atmospheres surrounding elliptical galaxiesand BCGs, it is able to sweep higher density molecular gas away from theircenters.

A $10^{10}$ Solar Mass Flow of Molecular Gas in the Abell 1835 Brightest Cluster Galaxy