Late-Time Optical and Ultraviolet Spectra of SN 1979C and SN 1980K
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CitationFesen, Robert A., Christopher L. Gerardy, Alexei V. Filippenko, Thomas Matheson, Roger A. Chevalier, Robert P. Kirshner, Brian P. Schmidt, et al. 1999. “Late-Time Optical and Ultraviolet Spectra of SN 1979C and SN 1980K.” The Astronomical Journal 117 (2): 725–35. https://doi.org/10.1086/300751.
AbstractA low-dispersion Keck I spectrum of SN 1980K taken in 1995 August (t = 14.8 yr after explosion) and a spectrum taken in 1997 November (t = 17.0 yr) at the MDM Observatory show broad 5500 km s(-1) emission lines of H alpha, [O I] 6300, 6364 Angstrom, and [O II] 7319, 7330 Angstrom. Weaker but similarly broad lines detected include [Fe II] 7155 Angstrom,, [S II] 4068, 4072 Angstrom, and a blend of [Fe II] lines at 5050-5400 Angstrom. The presence of strong [S II] 4068, 4072 Angstrom emission but a lack of [S II] 6716, 6731 Angstrom emission suggests electron densities of 10(5)-10(6) cm(-3) From the 1997 spectrum, we estimate an H alpha flux of (1.3 +/- 0.2) x 10(-15) ergs cm(-2) s(-1), indicating a 25% decline from the 1987-1992 levels during the period 1994 to 1997, possibly related to a reported decrease in its nonthermal radio emission. A 1993 May, Multiple Mirror Telescope spectrum of SN 1979C (t = 14.0 yr) shows a somewhat different spectrum from that of SN 1980K. Broad, 6000 km s(-1) emission lines are also seen but with weaker H alpha, stronger [O III] 4959, 5007 Angstrom, more highly clumped [O I] and [O II] line profiles, no detectable [Fe II] 7155 Angstrom emission, and a faint but very broad emission feature near 5750 Angstrom. A 1997 Hubble Space Telescope Faint Object Spectrograph, near-UV spectrum (2200-4500 Angstrom) shows strong lines of C II] 2324, 2325 Angstrom, [O II] 2470 Angstrom, and Mg II 2796, 2803 Angstrom, along with weak [Ne III] 3969 Angstrom [S II] 4068, 4072 Angstrom, and [O III] 4363 Angstrom emissions. The UV emission lines show a double-peak profile with the blueward peak substantially stronger than the red, suggesting dust extinction within the expanding ejecta CE(B-V)= 0.11-0.16 mag]. The lack of detectable [O II] 3726, 3729 Angstrom emission, together with [O III] lambda lambda(4959 + 5007)/lambda 4363 similar or equal to 4, implies electron densities 10(6)-10(7) cm(-3). These Type II linear supernovae (SNe II-L) spectra show general agreement with the lines expected in a circumstellar interaction model, but the specific models that are available show several differences with the observations. High electron densities (10(5)-10(7) cm(-3)) result in stronger collisional de-excitation than assumed in the models, thereby explaining the absence of several moderate to strong predicted lines such as [O II] 3726, 3729 Angstrom, [N II] 6548, 6583 Angstrom, and [S II] 6716, 6731 Angstrom. Interaction models are needed that are specifically suited to these supernovae. We review the overall observed range of late-time SNe II-L properties and briefly discuss their properties relative to young, ejecta-dominated Galactic supernova remnants.
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