Astronomy and Astrophysics – Astronomy
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.8505d&link_type=abstract
American Astronomical Society, 194th AAS Meeting, #85.05; Bulletin of the American Astronomical Society, Vol. 31, p.973
Astronomy and Astrophysics
Astronomy
2
Scientific paper
The ultra-luminous supernova remnant (SNR) in NGC 6946 is the brightest X-ray SNR known, ~ 1000 times as luminous as Cas A. However, high-velocity gas with Vexp > 600 km/s has not been detected, as expected for a young remnant. HST WFPC2 images of this SNR show multiple loops. This morphology has been used as evidence of colliding SNRs of different ages, in order to explain the X-ray luminosity (Blair, Fesen, & Schlegel 1997), We have obtained high-dispersion echelle spectra of this SNR with the KPNO 4-m telescope. The SNR is detected in Hα , [N II]lambda 6584, and [O III]lambda 5007 lines. The emission lines show a narrow component (FWHM ~ 40 km/s) superposed on a broad component (FWZI ~ 360 km/s). The total [N II] flux is comparable to the Hα flux. The broad component contains ~ 1.5 times as much flux as the narrow component, and the broad component has slightly higher [N II]/Hα ratio than the narrow component. These spectral properties are qualitatively similar to some small SNRs in M33. The strong [N II] line in the narrow component suggests an anomalous nitrogen abundance usually associated with circumstellar material. The nitrogen abundance and small remnant size imply that the supernova progenitor was a WN star and the supernova exploded in a dense circumstellar bubble.
Chu Y.-H. Y.-H.
Dunne Bryan C.
Gruendl Robert A.
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