Astron. Astrophys. Suppl. Ser. 144, 219-225
Q.-Z. Liu1,2,3 - J.-Y. Hu4 - H.-R. Hang1 - Y.-L. Qiu2,4 - Z.-X. Zhu1 - Q.-Y. Qiao2,4
Send offprint request: Q.-Z. Liu, e-mail: email@example.com
1 - Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
2 - National Astronomical Observatories, Chinese Academy of Sciences, China
3 - Astronomical Institute, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
4 - Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Received January 3; accepted February 17, 2000
The spectral evolution is typical for SN II-L, very similar to that of the SN 1979C. They, however, showed some differences. The spectrum before maximum showed high-ionization N III and He II emission lines superposed on a strong blue continuum. Around the maximum light the high-ionization emission lines disappeared, leaving weak H I, He I emission lines, which are similar to those of SN 1983K. The extraordinary feature on the post-maximum spectra is the narrow emission P Cygni profile superposed on a much broader P Cygni structure in all five Balmer lines, H to H. Such feature is reminiscent of the post-maximum spectra of SN 1984E.
Rapid spectral and photometric evolution, together with the presence of obvious P Cygni profile, suggests that SN 1998S is more consistent with the nature of a type II-L supernova than that of a IIn supernova, although narrow lines are present on the premaximum spectrum.
Key words: supernovae: general -- supernovae: individual (SN 1998S)
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