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We report the discovery of a powerful molecular wind from the nucleus of thenon-interacting nearby S0 field galaxy NGC 1266. The single-dish CO profileexhibits emission to +/- 400 km/s and requires a nested Gaussian fit to beproperly described. Interferometric observations reveal a massive, centrally-concentrated molecular component with a mass of 1.1x10^9 Msuns and a molecularoutflow with a molecular mass of 2.4x10^7 Msuns. The molecular gas close to thesystemic velocity consists of a rotating, compact nucleus with a mass of about4.1x108 Msuns within a radius of approximately 60 pc. This compact molecularnucleus has a surface density of \approx 2.7 \times 10^4 Msuns/pc^2, more thantwo orders of magnitude larger than that of giant molecular clouds in the diskof the Milky Way, and it appears to sit on the Kennicutt-Schmidt relationdespite its extreme kinematics and energetic activity. We interpret thisnucleus as a disk that confines the outflowing wind. A mass outflow rate of 13Msuns/yr leads to a depletion timescale of about 85 Myr. The star formation inNGC 1266 is insufficient to drive the outflow, and thus it is likely driven bythe active galactic nucleus (AGN). The concentration of the majority of themolecular gas in the central 100 pc requires an extraordinary loss of angularmomentum, but no obvious companion or interacting galaxy is present to enablethe transfer. NGC 1266 is the first known outflowing molecular system that doesnot show any evidence of a recent interaction.

Discovery of an AGN-Driven Molecular Outflow in the Local Early-Type Galaxy NGC 1266