ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection
ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection
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DOI：
10.1093/mnras/stab2506
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发表时间：
2021-05
影响因子：
4.8
通讯作者：
K. Murase;C. Omand;D. Coppejans;H. Nagai;G. Bower;R. Chornock;D. Fox;K. Kashiyama;C. Law;R. Margutti;P. Mészáros
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作者：
K. Murase;C. Omand;D. Coppejans;H. Nagai;G. Bower;R. Chornock;D. Fox;K. Kashiyama;C. Law;R. Margutti;P. Mészáros
快速旋转的磁星和磁星被认为是超亮超新星（SLSNe）和快速射电爆发的中心引擎，这种情况自然预测了它们新生的脉冲星风星云（PWNe）的非热同步辐射。本文报道了用阿尔马和NOEMA对三个SLSNe（SN 2015 bn，SN 2016 ard和SN 2017 egm）的高频射电观测结果，并提出了一个详细的理论模型来计算来自PWNe的非热辐射，其年龄为101 −3年。我们发现，阿尔马数据不利于PWN模型的蟹状星云SN 2015 bn和SN 2017 egm的动机，并认为，这种紧张局势可以解决，如果星云的磁化是非常高或非常低。这种模型可以通过未来的MeV-GeV伽马射线望远镜（如AMEGO）进行测试。
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.