Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21430902s&link_type=abstract
American Astronomical Society, AAS Meeting #214, #309.02; Bulletin of the American Astronomical Society, Vol. 41, p.738
Astronomy and Astrophysics
Astronomy
Scientific paper
The star KPD0005+5106 is the hottest known helium-rich white dwarf. Until recently, its best-fit effective temperature was 120,000 K. This rose to 200,000 K with the identification of Ne VIII features in its UV and optical spectra (Werner et al. 2007, A&A, 474, 591). The star is surrounded by an [O III] lambda5007 emitting nebula about 3 degrees across (Chu et al. 2004, AJ, 128, 2357). Closer in, at angular distances between 1.7 and 3.5 arcminutes from the star, bright O VI lambda1032 emission has been detected in Far Ultraviolet Spectroscopic Explorer (FUSE) spectra (Otte et al. 2004, ApJL, 606, 134). Chu et al. argue that, because of its enormous mass (about 70 solar masses), the optical nebula consists of interstellar material, while Otte et al. suggest, based on the properties of the white dwarf and the spatial scale of the emission, that the O VI arises from photoionization by the central star of material in a planetary nebula. Since then, the upward revision of the effective temperature has changed both its inferred ionizing spectrum and its distance from us. We have also obtained additional FUSE observations of the region around the white dwarf.
We present the complete set of FUSE observations of the O VI-emitting nebula around KPD0005+5106, reduced with the latest version of the FUSE calibration pipeline. Using the most recent best-fit atmosphere model for the white dwarf atmosphere, we calculate photoionization models to interpret the O VI emission-line data. The increased distance to the white dwarf and its higher temperature suggest that the O VI-emitting material is part of the interstellar medium. The presence of O VI also places limits on the amount of material between the emitting region and KPD0005+5106 that may have been ejected by the star.
This work is supported by USRA.
Dixon William V.
Sankrit Ravi
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