论文标题
十年旧I型超浮肿超新星的无线电排放，PTF10HGI：与FRB121102进行比较
Radio emission from a decade old Type I superluminous supernova, PTF10hgi: Comparison with FRB121102
论文作者
论文摘要
我们在唯一的无线电检测到的I型超小型超新星（SLSN）PTF10HGI与最活跃的重复快速无线电爆发FRB121102之间进行了比较研究。这项研究的根源是假设的FRB-SLSN连接，该连接指出SLSN中出生的磁铁可以为FRB供电。此处介绍的PTF10HGI的宽带光谱（0.6--15 GHz）为无线电发射的磁性风膜起源提供了有力的证据。相同的光谱还使我们能够对无线电发射区域的半径和磁场进行稳健的估计，并证明星云由磁力的旋转能提供动力。然后将此频谱与FRB121102的频谱进行比较，我们使用档案数据将其延伸至400 MHz。新添加的测量结果对与FRB121102相关的紧凑型持续源的发射模型非常严格。我们发现，尽管两个来源都可以由基础磁体的旋转能提供动力，但在FRB121102中，平均能量注入速率要高得多。因此，我们假设，如果PTF10HGI确实在发射快速无线电爆发，那么它们的能量将比FRB121102的能量弱得多。
We perform a comparative study between the only radio detected Type I superluminous supernova (SLSN) PTF10hgi, and the most active repeating fast radio burst FRB121102. This study has its root in the hypothesized FRB-SLSN connection that states that magnetars born in SLSN can power FRBs. The wideband spectrum (0.6--15 GHz) of PTF10hgi presented here, provides strong evidence for the magnetar wind nebular origin of the radio emission. The same spectrum also enables us to make robust estimates of the radius and the magnetic field of the radio emitting region and demonstrates that the nebula is powered by the rotational energy of the magnetar. This spectrum is then compared with that of FRB121102 which we extend down to 400 MHz using archival data. The newly added measurements put very tight constraint on the emission models of the compact persistent source associated with FRB121102. We find that while both sources can be powered by the rotational energy of the underlying magnetar, the average energy injection rate is much higher in FRB121102. Hence, we hypothesise that, if PTF10hgi is indeed emitting fast radio bursts, those will be much weaker energetically than those from FRB121102.
