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Title: Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d

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 ≳ 104K and L ≲ 104L⊙. Additionally, we do not see any evidence for narrow H α emission inmore » our spectrum. We conclude that observations continue to strongly exclude many single-degenerate scenarios for SN 2011fe.« less

Authors:
 [1];  [2];  [3];  [1];  [4];  [5];  [1];  [1]
+ Show Author Affiliations
  1. Univ. of California, Berkeley, CA (United States)
  2. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  3. Univ. of Southampton (United Kingdom)
  4. Univ. of Maryland, College Park, MD (United States); NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
  5. Univ. of Texas, Austin, TX (United States)
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR)
OSTI Identifier:
1512132
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 454; Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Graham, M. L., Nugent, P. E., Sullivan, M., Filippenko, A. V., Cenko, S. B., Silverman, J. M., Clubb, K. I., and Zheng, W. Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d. United States: N. p., 2015. Web. doi:10.1093/mnras/stv1888.
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Graham, M. L., Nugent, P. E., Sullivan, M., Filippenko, A. V., Cenko, S. B., Silverman, J. M., Clubb, K. I., & Zheng, W. Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d. United States. https://doi.org/10.1093/mnras/stv1888
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Graham, M. L., Nugent, P. E., Sullivan, M., Filippenko, A. V., Cenko, S. B., Silverman, J. M., Clubb, K. I., and Zheng, W. Fri . "Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d". United States. https://doi.org/10.1093/mnras/stv1888. https://www.osti.gov/servlets/purl/1512132.
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@article{osti_1512132,
title = {Constraining the progenitor companion of the nearby Type Ia SN 2011fe with a nebular spectrum at +981 d},
author = {Graham, M. L. and Nugent, P. E. and Sullivan, M. and Filippenko, A. V. and Cenko, S. B. and Silverman, J. M. and Clubb, K. I. and Zheng, W.},
abstractNote = {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 ≳ 104K and L ≲ 104L⊙. 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.},
doi = {10.1093/mnras/stv1888},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 454,
place = {United States},
year = {Fri Oct 09 00:00:00 EDT 2015},
month = {Fri Oct 09 00:00:00 EDT 2015}
}
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Journal Article:
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Publisher's Version of Record
https://doi.org/10.1093/mnras/stv1888
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Cited by: 41 works
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Figures / Tables:

Figure 1 Figure 1: Images from Keck+LRIS on 2014 May 25 in the LRIS g and RS filters (left and right, respectively). Pixels have been grey-scaled to show the faint SN 2011fe (circle) in a field crowded by brighter sources and contaminated by diffuse background light from M101. The blue box representsmore » the slit width and orientation used for the Keck+LRIS spectrum obtained on 2014 May 1, and the size of the circles is set equal to the full width of the aperture used to extract the 1-dimensional spectrum. Despite the crowded field, our slit width, orientation, and chosen aperture limit contamination from nearby stars.« less
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