ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection
Abstract
Fast-rotating pulsars and magnetars have been suggested as the central engines of superluminous supernovae (SLSNe) and fast radio bursts, and this scenario naturally predicts non-thermal synchrotron emission from their nascent pulsar wind nebulae (PWNe). We report results of high-frequency radio observations with ALMA and NOEMA for three SLSNe (SN 2015bn, SN 2016ard, and SN 2017egm), and present a detailed theoretical model to calculate non-thermal emission from PWNe with an age of ∼1−3 yr. We find that the ALMA data disfavours a PWN model motivated by the Crab nebula for SN 2015bn and SN 2017egm, and argue that this tension can be resolved if the nebular magnetization is very high or very low. Such models can be tested by future MeV–GeV gamma-ray telescopes such as AMEGO.
Additional Information
© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 August 24. Received 2021 August 21; in original form 2021 May 12. Published: 07 September 2021. The ALMA observations were performed based on the Cycle 5 ALMA proposal with the project code 2017.1.00975.S, titled with 'Searching for the Smoking Gun of Magnetar-Powered Super-Luminous Supernovae' (PI: Kohta Murase) and the Cycle 6 ALMA proposal with the project code 2018.1.01295.S, titled with 'A Direct Test of the Magnetar-Model in SLSNe' (PI: Deanne Coppejans). ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The NOEMA observations were performed based on the Summer 2018 NOEMA proposal with the project ID S18BH, titled 'Testing the Magnetar-Powered Scenario for Super-Luminous Supernovae with NOEMA' (PI: Conor Omand). The work of KM is supported by the Alfred P. Sloan Foundation, NSF Grant nos AST-1908689, AST-2108466, AST-2108467, and KAKENHI nos 20H01901 and 20H05852. CMBO has been supported by the Grant-in-aid for the Japan Society for the Promotion of Science (18J21778). The authors would like to thank Michel Bremer and Jan Martin Winters for their help with NOEMA data reduction. Data Availability: The ALMA data presented in this paper are available at the ALMA archive using the project codes 2017.1.00975.S (PI: Kohta Murase) and 2018.1.01295.S (PI: Deanne Coppejans). The NOEMA data can be found the IRAM archive using the project ID S18BH001 (PI: Conor Omand). The theoretical model data underlying this article will be shared on reasonable request to the corresponding author.Attached Files
Published - stab2506.pdf
Accepted Version - 2105.05239.pdf
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Additional details
- Eprint ID
- 111626
- Resolver ID
- CaltechAUTHORS:20211025-143630189
- Alfred P. Sloan Foundation
- AST-1908689
- NSF
- AST-2108466
- NSF
- AST-2108467
- NSF
- 20H01901
- Japan Society for the Promotion of Science (JSPS)
- 20H05852
- Japan Society for the Promotion of Science (JSPS)
- 18J21778
- Japan Society for the Promotion of Science (JSPS)
- Created
-
2021-10-26Created from EPrint's datestamp field
- Updated
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2021-10-26Created from EPrint's last_modified field