A transient radio source consistent with a merger-triggered core collapse supernova
Radio evidence of a stellar merger
Core collapse supernovae occur when a massive star exhausts its fuel and explodes. Theorists have predicted that a similar explosion could occur if an evolved massive star merges with a compact companion, such as a neutron star. Dong et al. have identified a radio source that was not present in earlier radio surveys. Follow-up radio and optical spectroscopy show that it is an expanding supernova remnant slamming into surrounding material, probably ejected from the star centuries before it exploded. An unidentified x-ray transient occurred at a consistent location in 2014, suggesting an explosion at that time that produced a jet. The authors suggest that the most likely explanation is a merger-triggered supernova. —KTS
Abstract
A core collapse supernova occurs when exothermic fusion ceases in the core of a massive star, which is typically caused by exhaustion of nuclear fuel. Theory predicts that fusion could be interrupted earlier by merging of the star with a compact binary companion. We report a luminous radio transient, VT J121001+495647, found in the Very Large Array Sky Survey. The radio emission is consistent with supernova ejecta colliding with a dense shell of material, potentially ejected by binary interaction in the centuries before explosion. We associate the supernova with an archival x-ray transient, which implies that a relativistic jet was launched during the explosion. The combination of an early relativistic jet and late-time dense interaction is consistent with expectations for a merger-driven explosion.
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Volume 373 | Issue 6559
3 September 2021
3 September 2021
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Copyright © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.
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Submission history
Received: 15 January 2021
Accepted: 3 August 2021
Published in print: 3 September 2021
Acknowledgments
We thank the NRAO staff who made the VLASS possible, the VLASS Survey Science Group, J. Fuller and J. Lux for useful discussions, and the reviewers for helpful comments. Our results are based on data from the Karl G. Jansky Very Large Array, which is operated by the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities Inc. This research has made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. Some of the data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize and acknowledge the cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding: D.Z.D. and G.H. were supported by National Science Foundation (NSF) grant AST-1654815. G.H., D.Z.D., and A.H. were supported by the United States–Israel Binational Science Foundation (grant 2018154). A.H. also acknowledges support from the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation and ISF grant 647/18. A.Y.Q.H. and K.D. were supported by the GROWTH project funded by the NSF under PIRE grant 1545949. A.K.H. was supported by NSERC Discovery Grants RGPIN-2016-06569 and RGPIN-2021-04001. A.Y.Q.H. was supported by the Miller Institute for Basic Research in Science at the University of California, Berkeley. K.H. was supported by JSPS Early-Career Scientists grant 20K14513. S.M. was supported by the NRAO. S.R.K. was supported by the Heising-Simons Foundation. Author contributions: G.H., D.Z.D., and K.P.M. designed the transient search strategy. D.Z.D. implemented the transient search pipeline, with help from A.K.H. in visual vetting and A.Y.Q.H. in matching the MAXI transient. D.Z.D., G.H., and S.T.M. obtained the radio and optical follow-up observations with the help of telescope staff at the VLA and Keck. D.Z.D. processed and analyzed the radio data with contributions from S.T.M. D.Z.D. processed and analyzed the optical data and estimated the transient rates. E.N. led the analysis of the x-ray data with help from D.Z.D. D.Z.D. and G.H. wrote the paper with contributions from E.N., K.H., and the remaining authors. Competing interests: The authors declare no competing interests. Data and materials availability: VLASS quicklook images are available at https://archive-new.nrao.edu/vlass/quicklook/. VLA follow-up observations are available from the VLA archive at https://archive.nrao.edu/ under project code 19A-422. The FIRST data were taken from https://third.ucllnl.org/cgi-bin/firstcutout. The Keck observations are available at https://koa.ipac.caltech.edu/cgi-bin/KOA/nph-KOAlogin?more with KOAIDs beginning LB.20180413. The Hubble Space Telescope image was taken from the archive https://hla.stsci.edu/ under proposal ID 13493. Our analysis and model fitting software code is available at https://github.com/Dillon-Z-Dong/VT1210 and is archived on Zenodo (38).
Authors
Funding Information
National Science Foundation: AST-1654815
National Science Foundation: PIRE Grant No. 1545949
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