O VI Emission from NGC7009, the Saturn Nebula.

Details O VI Emission from NGC7009, the Saturn Nebula. O VI Emission from NGC7009, the Saturn Nebula.

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.8915i&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #89.15; Bulletin of the American Astronomical Society, Vol. 34, p.1254

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We present far-ultraviolet 905-1187 Å spectroscopy of the Saturn Nebula, NGC 7009, obtained with the FUSE satellite. To isolate the nebula from the central star, the narrow slit, 1.25 x 20 arcsec, of the FUSE instrument was used and positioned at two different locations in the nebula. FUSE detected nebular O VI 1032, 1038 Å emission lines at both locations in the nebula, with a stronger emission at the location closest to the central star. O VI is the dominant cooling agent for gas at T ~ 3 x 105 K. Emission lines of He II, C III, N II, S III, S IV, and Si IV are also present. A FUSE observation of the central star reveals a very strong O VI 1032-1038 Å P-Cygni line profile with a terminal velocity of ~ 3000 km/sec. Financial support has been provided by NASA grant NAG5-12347 to CUA.

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