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.

中文翻译：

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ALMA 和 NOEMA 对来自胚胎超光超新星遗迹的同步加速器星云发射和射电伽马射线连接的约束

快速旋转的脉冲星和磁星被认为是超亮超新星 (SLSNe) 和快速射电暴的中心引擎，这种情况自然地预测了它们新生的脉冲星风星云 (PWNe) 的非热同步辐射。我们报告了三个 SLSNe（SN 20150 亿、SN 2016ard 和 SN 2017egm）的 ALMA 和 NOEMA 高频射电观测结果，并提出了一个详细的理论模型来计算年龄约为 1-3 岁的 PWNe 的非热发射年。我们发现 ALMA 数据不支持由蟹状星云推动的 SN 20150 亿和 SN 2017egm 的 PWN 模型，并认为如果星云磁化强度非常高或非常低，这种张力可以得到解决。此类模型可以通过未来的 MeV-GeV 伽马射线望远镜（如 AMEGO）进行测试。