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The chemical composition of PNG 135.9+55.9, the most oxygen poor planetary nebula

Published online by Cambridge University Press:  23 December 2005

Grażyna Stasińska ,
G. H. Tovmassian ,
M. G. Richer ,
M. Peña ,
R. Napiwotzki ,
C. Charbonnel  and
L. Jamet
Grażyna Stasińska
Affiliation:
LUTH, Observatoire de Meudon, 92195 Meudon Cedex, France email: [email protected]
G. H. Tovmassian
Affiliation:
Observatorio Astronómico Nacional, Instituto de Astronomía, UNAM, P.O. Box 439027, San Diego, CA 92143-9027, USA
M. G. Richer
Affiliation:
Observatorio Astronómico Nacional, Instituto de Astronomía, UNAM, P.O. Box 439027, San Diego, CA 92143-9027, USA
M. Peña
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 70 264, México D.F., 04510, México
R. Napiwotzki
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hatfield, AL10 9AB, UK
C. Charbonnel
Affiliation:
Geneva Observatory, 51 Chemin des Maillettes, CH 1290 Sauverny
L. Jamet
Affiliation:
LUTH, Observatoire de Meudon, 92195 Meudon Cedex, France email: [email protected]
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Abstract

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PN G 135.9 +55.9 is an extraordinary nebula discovered recently in the Galactic halo (Tovmassian et al. 2001). The first studies estimated its oxygen abundance to be 1/100 of the solar value or even less.

Being extremely metal-poor, PNG 135.9+55.9 offers an unprecedented opportunity to check our understanding of the evolution of intermediate-mass stars at very low metallicity, by complementing the data obtained from metal-poor giants (Spite et al 2005). Indeed, PNG 135.9+55.9 and some of those stars are snapshots of the evolution of very similar stars at different times.

We present our most recent abundance analysis for this object, providing stringent limits on the abundances of C, N, O, and Ne, to be confronted with the predictions for the yields of low metallicity intermediate mass stars.

Keywords

ISM: planetary nebulae: individual (PNG 135.9+55.9)stars: AGB and post-AGBstars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 323 - 326
Copyright
© 2005 International Astronomical Union