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Constraining the Progenitor Companion of the Nearby Type Ia SN 2011fe with a Kiloday Nebular Spectrum | Melissa L. Graham
; Peter E. Nugent
; Mark Sullivan
; Alexei V. Filippenko
; S. Bradley Cenko
; Jeffrey M. Silverman
; Kelsey I. Clubb
; Weikang Zheng
; | Date: |
26 Jan 2015 | Abstract: | We present a "kiloday" optical nebular spectrum of the nearby Type Ia
supernova (SN) 2011fe, obtained +981 days after explosion. SN 2011fe exhibits
little evolution since the +593 day optical spectrum, but there are several
curious aspects in this new extremely late-time regime. We see new emission
features at 5800 and 6400 AA that could be attributed to [Fe I], but also
consider (and reject) the possibility that the latter is the high-velocity
hydrogen predicted by Mazzali et al. (2014). The nebular feature at 5200 AA
exhibits a linear velocity evolution of $sim350$ $
m km s^{-1}$ per 100 days
from at least +220 to +980 days, but the line’s shape also changes in this
time, suggesting that line blending contributes to the evolution. At $sim
1000$ days after explosion, flux from the SN has declined to a point where
contribution from a hot, luminous secondary could be detected. In this work we
make the first observational tests for a post-impact remnant star and constrain
its luminosity to $<(3-5) imes 10^3$ $
m L_{odot}$. Additionally, we do not
see any evidence for narrow H$alpha$ emission, placing an upper limit of $3
imes 10^{-4}$ $
m M_{odot}$ on the mass of hydrogen in the system. We
conclude that observations continue to strongly exclude many single-degenerate
scenarios for SN 2011fe. | Source: | arXiv, 1502.0646 | Services: | Forum | Review | PDF | Favorites |
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