Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig
Abstract
We present HST/WFC3 ultraviolet imaging in the F275W and F336W bands of the Type IIb SN 2001ig at an age of more than 14 years. A clear point source is detected at the site of the explosion, with m_(F275W) = 25.39 ± 0.10 and m_(F336W) = 25.88 ± 0.13 mag. Despite weak constraints on both the distance to the host galaxy NGC 7424 and the line-of-sight reddening to the supernova, this source matches the characteristics of an early B-type main-sequence star with 19,000 < T_(eff) < 22,000 K and log(L_(bol)/L⊙) = 3.92 ± 0.14. A BPASS v2.1 binary evolution model, with primary and secondary masses of 13 M⊙ and 9 M⊙, respectively, is found to simultaneously resemble, in the Hertzsprung–Russell diagram, both the observed location of this surviving companion, and the primary star evolutionary endpoints for other Type IIb supernovae. This same model exhibits highly variable late-stage mass loss, as expected from the behavior of the radio light curves. A Gemini/GMOS optical spectrum at an age of 6 years reveals a narrow He II λ4686 emission line, indicative of continuing interaction with a dense circumstellar medium at large radii from the progenitor. We review our findings on SN 2001ig in the context of binary evolution channels for stripped-envelope supernovae. Owing to the uncrowded nature of its environment in the ultraviolet, this study of SN 2001ig represents one of the cleanest detections to date of a surviving binary companion to a Type IIb supernova.
Additional Information
© 2018 The American Astronomical Society. Received 2017 October 4; revised 2018 January 15; accepted 2018 February 8; published 2018 March 27. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support was provided by NASA through grants GO-14075 and AR-14295 from STScI. It is also based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). We thank the referee for their suggestions, and are grateful to J. J. Eldridge for discussions regarding the BPASS models. A.V.F.'s group is also grateful for generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST-1211916, and the Miller Institute for Basic Research in Science (U.C. Berkeley). E.Z. is supported by a grant of the Netherlands Research School for Astronomy (NOVA). S.d.M. acknowledges support by a Marie Sklodowska-Curie Action (H2020 MSCA-IF-2014, project BinCosmos, id 661502).Attached Files
Published - Ryder_2018_ApJ_856_83.pdf
Submitted - 1801.05125.pdf
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Additional details
- Eprint ID
- 85470
- Resolver ID
- CaltechAUTHORS:20180327-160323727
- NAS 5-26555
- NASA
- GO-14075
- NASA
- AR-14295
- NASA
- Christopher R. Redlich Fund
- TABASGO Foundation
- AST-1211916
- NSF
- University of California, Berkeley
- Nederlandse Onderzoekschool Voor Astronomie (NOVA)
- 661502
- Marie Sklodowska-Curie Action
- Created
-
2018-03-28Created from EPrint's datestamp field
- Updated
-
2021-11-15Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)