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Unravelling the chemical inhomogeneity of PNe with VLT FLAMES integral-field unit spectroscopy

Published online by Cambridge University Press:  15 December 2006

Y. G. Tsamis ,
J. R. Walsh ,
D. Péquignot ,
M. J. Barlow ,
X.-W. Liu  and
I. J. Danziger
Y. G. Tsamis
Affiliation:
Dept. of Physics & Astronomy, University College London, London WC1E 6BT, U. K.
J. R. Walsh
Affiliation:
European Southern Observatory, D-85748 Garching, Germany
D. Péquignot
Affiliation:
LUTH, Observatoire de Meudon-Paris, F-92195 Meudon, France
M. J. Barlow
Affiliation:
Dept. of Physics & Astronomy, University College London, London WC1E 6BT, U. K.
X.-W. Liu
Affiliation:
Dept. of Astronomy, Peking University, Beijing, China
I. J. Danziger
Affiliation:
Osservatorio di Trieste, I-34131 Trieste, Italy
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Abstract

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Recent weak emission-line long-slit surveys and modelling studies of PNe have convincingly argued in favour of the existence of an unknown component in the planetary nebula plasma consisting of cold, hydrogen-deficient gas, as an explanation for the long-standing recombination-line versus forbidden-line temperature and abundance discrepancy problems. Here we describe the rationale and initial results from a detailed spectroscopic study of three Galactic PNe undertaken with the VLT FLAMES integral-field unit spectrograph, which advances our knowledge about the small-scale physical properties, chemical abundances and velocity structure of these objects across a two-dimensional field of view, and opens up for exploration an uncharted territory in the study and modelling of PNe and photoionized nebulae in general.

Keywords

planetary nebulae: individual (NGC 5882, NGC 6153, NGC 7009)ISM: abundancesline: profiles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 239 - 242
Copyright
© 2006 International Astronomical Union