EDP Sciences
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Volume 376, Number 2, September II 2001
Page(s) 484 - 488
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20010922

A&A 376, 484-488 (2001)
DOI: 10.1051/0004-6361:20010922

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

E. Josselin1 and R. Bachiller2

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

(Received 27 April 2001 / 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 ${\sim} 10^{-4} M_{\odot}$. 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 ( ${\sim}2.4\times10^4$ 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.

Key words: planetary nebulae: general -- planetary nebulae: individual: BV 5-1 -- radio lines: ISM -- stars: mass loss

Offprint request: E. Josselin, josselin@graal.univ-montp2.fr

SIMBAD Objects in preparation

© ESO 2001