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Far Ultraviolet Emission from NGC 7009

Published online by Cambridge University Press:  15 December 2006

R. C. Iping ,
G. Sonneborn ,
S. R. McCandliss  and
Y-H. Chu
R. C. Iping
Affiliation:
The Catholic University of America, Washington, DC 20064, USA email: iping@milkyway.gsfc.nasa.gov NASA/GSFC, Code 665, Greenbelt MD 20771, USA
G. Sonneborn
Affiliation:
NASA/GSFC, Code 665, Greenbelt MD 20771, USA
S. R. McCandliss
Affiliation:
Dept. of Physics and Astronomy, The Johns Hopkins Univ, Baltimore MD 21218, USA
Y-H. Chu
Affiliation:
Dept. of Astronomy, Univ. of Illinois, Urbana, IL 61801, USA
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Abstract

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The high-excitation planetary nebula NGC 7009 and its central star were observed with the Far Ultraviolet Spectroscopic Explorer (FUSE) through a 30$\,{\times}\,$30 arcsec (LWRS) aperture, and with the HIRS narrow slit (1.25$\,{\times}\,$20 arcsec) to isolate the inner and outer parts of the nebula from the central star. The high-resolution (15 km/s) nebular spectra (910-1187 Å) show strong emission from C III] and permitted transitions of He II N II, N III, S III, S IV, S VI and O VI, with stronger emission closer to the central star. In this paper we present results obtained on the spatial variation of these tracers of highly ionized gas. The hot central star of NGC 7009 is discussed in a separate paper by Sonneborn et al.

Keywords

planetary nebulae: individual (NGC 7009)ultraviolet: starstechniques: spectroscopicline: identificationspace vehicles: FUSE
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 429 - 430
Copyright
© 2006 International Astronomical Union