Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d. Issue 2 (9th October 2015)

• Record Type: Journal Article
• Authors: Graham, M. L.; Nugent, P. E.; Sullivan, M.; Filippenko, A. V.; Cenko, S. B.; Silverman, J. M.; Clubb, K. I.; Zheng, W.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 454:Issue 2(2015)
• Page Start: 1948
• Page End: 1957
• Publication Date: 2015-10-09
• Subjects: supernovae: general -- supernovae: individual: SN 2011fe; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stv1888
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract : We present an optical nebular spectrum of the nearby Type Ia supernova 2011fe, obtained 981 d after explosion. SN 2011fe exhibits little evolution since the +593 d optical spectrum, but there are several curious aspects in this new extremely late-time regime. We suggest that the persistence of the ∼5800 Å feature is due to Na I D, and that a new emission feature at ∼7300 Å may be [Ca II]. Also, we discuss whether the new emission feature at ∼6400 Å might be [Fe I] or the high-velocity hydrogen predicted by Mazzali et al. The nebular feature at 5200 Å exhibits a linear velocity evolution of ∼350 km s − 1 per 100 d from at least +220 to +980 d, but the line's shape also changes in this time, suggesting that line blending contributes to the evolution. At ∼1000 d after explosion, flux from the SN has declined to a point where contribution from a luminous secondary could be detected. In this work, we make the first observational tests for a post-impact remnant star and constrain its temperature and luminosity to T ≳ 10 4 K and L ≲ 10 4 L⊙ . Additionally, we do not see any evidence for narrow H α emission in our spectrum. We conclude that observations continue to strongly exclude many single-degenerate scenarios for SN 2011fe.