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We have imaged in CO(2-1) the molecular gas in NGC 1275 (Perseus A), the cDgalaxy at the center of the Perseus Cluster, at a spatial resolution of $\sim$1kpc over a central region of radius $\sim$ 10 kpc. Per A is known to contain$\sim$1.3x10$^{10}$ M$_\odot$ of molecular gas, which has been proposed to becaptured from mergers with or ram-pressure stripping of gas-rich galaxies, oraccreted from a X-ray cooling flow. The molecular gas detected in our image hasa total mass of $\sim$4x10$^9$ M$_\odot$, and for the first time can be seen tobe concentrated in three radial filaments with lengths ranging from at least1.1-2.4 kpc all lying in the east-west directions spanning the center of thegalaxy to radii of $\sim$8 kpc. The eastern and outer western filaments exhibitlarger blueshifted velocities with decreasing radii, whereas the inner westernfilament spans the systemic velocity of the galaxy. The molecular gas shows nosignature of orbital motion, and is therefore unlikely to have been capturedfrom gas-rich galaxies. Instead, we are able to reproduce the observedkinematics of the two outer filaments as free-fall in the gravitationalpotential of Per A, as would be expected if they originate from a X-ray coolingflow. Indeed, all three filaments lie between two prominent X-ray cavitiescarved out by radio jets from Per A, and closely resembles the spatialdistribution of the coolest X-ray gas in the cluster core. The inferredmass-deposition rate into the two outermost filaments alone is roughly 75M$_odot$ yr$^{-1}$. This cooling flow can provide a nearly continuous supply ofmolecular gas to fuel the active nucleus in Per A.

Radially-Inflowing Molecular Gas in NGC 1275 Deposited by a X-ray Cooling Flow in the Perseus Cluster