A disrupted molecular ring in planetary nebula G119.3+00.3 (BV 5-1)*
GRAAL-CC72, UMR 5024-ISTEEM, CNRS/Univ. Montpellier II, 34095 Montpellier Cedex 05, France
2 Observatorio Astronómico Nacional (OAN), IGN, Apartado 1143, 28800 Alcalá de Henares, Spain
Corresponding author: E. Josselin, firstname.lastname@example.org
Accepted: 26 June 2001
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 are . 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 ~9 km s-1. BV 5-1 is confirmed to be a relatively evolved nebula, as indicated by both its kinematic age ( 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.
Key words: planetary nebulae: general / planetary nebulae: individual: BV 5-1 / radio lines: ISM / stars: mass loss
© ESO, 2001