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New, high-sensitivity interferometric CO observations of BV 5-1 show that the molecular gas in this bipolar planetary nebula is distributed along a very inhomogeneous ring made of clumps. The individual masses of such molecular clumps are10 4 M. The BV 5-1 molecular ring is seen edge-on, it is nearly perpendicular to the axis of bipolarity of the nebula, and it is expanding with an expansion velocity of 9k m s 1 .B V 5-1 is conrmed to be a relatively evolved nebula, as indicated by both its kinematic age (2:4 10 4 yrs) and its molecular to ionized mass ratio (0.3). The structure of the BV 5-1 molecular ring, as well as that of other rings previously observed in a few additional nebulae, underscore the importance of strongly asymmetrical mass loss processes starting early at the asymptotic giant branch phase.

A disrupted molecular ring in planetary nebula G119.3+00.3 (BV 5-1)