Discovery of Narrow O VI Emission from SN 1987A

Details Discovery of Narrow O VI Emission from SN 1987A Discovery of Narrow O VI Emission from SN 1987A

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.9504s&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #95.04; Bulletin of the American Astronomical Society, Vol. 34, p.956

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Scientific paper

O VI 1032, 1038 A emission from the circumstellar gas around SN 1987A has been detected in spectra obtained by the Far Ultraviolet Spectroscopic Explorer(FUSE) satellite. O VI is the highest ionization state yet detected in line emission from the SN 1987A circumstellar material. The O VI emission line profiles are narrow, with FWHM <35 km/sec, and have a heliocentric radial velocity of +280 km/sec. This places the emitting gas at rest relative to the supernova. Spectra obtained in Oct. 2000 and Sept. 2001 have essentially the same O VI fluxes. Simultaneous spectra obtained in the other FUSE apertures, positioned about 100 arcsec from SN 1987A, show nothing at the O VI wavelengths, eliminating diffuse emission in the LMC as a possible source of the O VI feature. The FUSE spectra of the two B-type stars near SN 1987A provide the line profiles of interstellar absorption on the sight lines within 3 arcsec of SN 1987A. The interstellar line profiles show that that intervening absorption has a negligible effect on the shape of the O VI emission. The narrow O VI emission probably originates from the H II region of very low density (n<100 /cm3) unshocked gas near the inner circumstellar ring that was ionized by the supernova outburst in 1987. It is unlikely that the narrow O VI emission is the result of recent reionization of circumstellar gas by X-rays produced by shock interactions. The observed O VI fluxes are in agreement with recombination models (Lundqvist 1999, ApJ, 511, 389) for the circumstellar material.

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