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Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap

Zapartas, E. and de Mink, S. E. and Van Dyk, S. D. and Fox, O. D. and Smith, N. and Bostroem, K. A. and de Koter, A. and Filippenko, A. V. and Izzard, R. G. and Kelly, P. L. and Neijssel, C. J. and Renzo, M. and Ryder, S. (2017) Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap. Astrophysical Journal, 842 (2). Art. No. 125. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170623-092526606

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Abstract

Many young, massive stars are found in close binaries. Using population synthesis simulations we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star >8–10 M⊙, ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially ≾23 M⊙. Although unlikely (<1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broad-lined Type Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern the evolution of SN progenitors.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa7467DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa7467/metaPublisherArticle
https://arxiv.org/abs/1705.07898arXivDiscussion Paper
ORCID:
AuthorORCID
de Mink, S. E.0000-0001-9336-2825
Van Dyk, S. D.0000-0001-9038-9950
Fox, O. D.0000-0003-2238-1572
Filippenko, A. V.0000-0003-3460-0103
Kelly, P. L.0000-0003-3142-997X
Additional Information:© 2017 The American Astronomical Society. Received 2017 March 7; revised 2017 May 17; accepted 2017 May 17; published 2017 June 22. We thank Jon Mauerhan, Isaac Shivvers, Jeff Silverman, Heechan Yuk, and WeiKang Zheng for contributing to the observing proposal. We are grateful to Ylva Götberg, Maryam Modjaz, Silvia Toonen, and Jacco Vink for very useful discussions. This work is based 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. It is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with NASA. Support was provided by NASA through grants GO-14075 and AR-14295 from STScI. We thank Andrew Dolphin for his patient advice on how best to implement artificial star tests in Dolphot. 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). A.V.F.'s group is also grateful for generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. N.S. is grateful for support from NSF grants AST-1312221 and AST-1515559. R.G.I. thanks the STFC for funding his Rutherford Fellowship under grant ST/L003910/1 and Churchill College, Cambridge, for his fellowship and access to their library. Software: AstroDrizzle, PyRAF, IRAF, TinyTim, DOLPHOT (v2.0; Dolphin 2000), MIST (Paxton et al. 2011, 2013, 2015; Choi et al. 2016), binary_c (version 2.0, SVN revision 4105; Izzard et al. 2004, 2006, 2009), Matplotlib (https://doi.org/10.1109/MCSE.2007.55).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS 5-26555
NASA/JPL/CaltechUNSPECIFIED
NASAGO-14075
NASAAR-14295
Nederlandse Onderzoekschool Voor Astronomie (NOVA)UNSPECIFIED
Marie Curie FellowshipH2020 MSCA-IF-2014
Christopher R. Redlich FundUNSPECIFIED
TABASGO FoundationUNSPECIFIED
NSFAST-1211916
NSFAST-1312221
NSFAST-1515559
Science and Technology Facilities Council (STFC)ST/L003910/1
Subject Keywords:binaries: close – binaries: general – stars: evolution – stars: massive – supernovae: general – supernovae: individual (SN 2002ap)
Issue or Number:2
Record Number:CaltechAUTHORS:20170623-092526606
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170623-092526606
Official Citation:E. Zapartas et al 2017 ApJ 842 125
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78508
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:26 Jun 2017 20:33
Last Modified:09 Mar 2020 13:19

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