ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection

Author:

Murase Kohta1234ORCID,Omand Conor M B5,Coppejans Deanne L6,Nagai Hiroshi78,Bower Geoffrey C910,Chornock Ryan11,Fox Derek B23,Kashiyama Kazumi512,Law Casey13,Margutti Raffaella12,Mészáros Peter123

Affiliation:

1. Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA

2. Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA

3. Center for Mulitmessenger Astrophysics, Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA

4. Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan

5. Department of Physics, Gradaute School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan

6. Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA); Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA

7. National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan

8. The Graduate University for Advanced Studies, SOKENDAI, Mitaka, Tokyo 181-8588, Japan

9. Academia Sinica Institute of Astronomy and Astrophysics, Hilo, HI 96720, USA

10. Department of Physics and Astronomy, University of Hawai’i at Mãnoa, Honolulu, HI 96822, USA

11. Astrophysical Institute; Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA

12. Research Center for the Early Universe; Department of Physics, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan

13. Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA

Abstract

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.

Funder

ESO

NINS

NRC

MOST

KASI

Alfred P. Sloan Foundation

NSF

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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