The Mystery of the Double-Peaked Emission Lines in Late-time Spectra of Core-Collapse SNe

Details The Mystery of the Double-Peaked Emission Lines in Late-time Spectra of Core-Collapse SNe The Mystery of the Double-Peaked Emission Lines in Late-time Spectra of Core-Collapse SNe

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008noao.prop..415f&link_type=abstract

NOAO Proposal ID #2008A-0415

Computer Science

Scientific paper

Late-time spectra of core-collapse SNe often show double-peaked line profiles in [O I] 6300,6364, Mg I] 4571, and [Ca II] 7291,7324. In a few cases, the double-peaked profile is seen blueshifted by 1000 - 2000 km/s. Such double-peaked line profiles have had widely different interpretations including ejecta rings, disks, jets, line blending, line opacities, and ejecta clumping. Whatever the correct explanation(s), recent late-time spectra of Type II, Ib, and Ic SNe have now made it clear that double-peaked line profiles are, in fact, very common - suggesting an important and unifying underlying characteristic may connect all core-collapse supernovae. Here we propose a Gemini N & S GMOS program of three recent and relatively bright Type II supernovae at ages of 200-350 days past maximum light that will yield better S/N and higher resolution spectra to better characterize the phenomena. These data will allow an accurate comparison for the expansion properties of O,Ne,Mg vs. S,Si,Ca rich ejecta zones through Mg I], O I, [O I], and [Ca II] line emissions. We will then examine the observed late-time emission properties using detailed core-collapse models.

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