论文标题
附近IA型超新星的最深无线电观察结果：约束祖细胞类型并优化未来的调查
The Deepest Radio Observations of Nearby Type IA Supernovae: Constraining Progenitor Types and Optimizing Future Surveys
论文作者
论文摘要
我们报告了附近的IA型超新星（SNE IA）的深度无线电观察结果，该观察结果具有电子多元素无线电链接的干涉仪网络（E-Merlin）和澳大利亚望远镜紧凑型阵列（ATCA）。未进行检测。使用相对论电子能量密度的标准假设进入幂律能量分布，并且磁场强度（Epsilon_e = Epsilon_b = 0.1），我们达到了SN 2013dy祖细胞系统的质量损失率的上限（2016COJ，2016COJ，2018GV，2018PV，2019NP），比12（2.8） 1.7）每年EE（-8）太阳能（以100 km/s的风速为止）。至Sne 2016coj，2018GV，2018PV和2019NP，我们为附近17个SNE IA添加了无线电数据，并为其非检测构建了建模。使用与所述的模型相同，所有21个IA的质量损失率每年低于4EE（-8）个太阳能（以100 km/s的风速）。我们将这些限制与不同的单位祖细胞场景中的预期质量损失率进行了比较。我们还讨论了如何从无线电中检测到的SNE IA和最年轻的SN IA残留物以及剥离的Envelope Core-Collapse SNE中检测到的SNNE IA和最年轻的SN IA残留物的信息。我们突出显示了SN 2011DH，并主张EPSILON_E大约等于0.1，而EPSILON_B大约等于0.0033。最后，考虑到自爆炸以来的时间，与超新星和望远镜灵敏度的距离，我们讨论了在无线电频率上观察以最大化检测机会的策略。
We report deep radio observations of nearby Type Ia Supernovae (SNe Ia) with the electronic Multi-Element Radio Linked Interferometer Net-work (e-MERLIN), and the Australia Telescope Compact Array (ATCA). No detections were made. With standard assumptions for the energy densities of relativistic electrons going into a power-law energy distribution, and the magnetic field strength (epsilon_e = epsilon_B = 0.1), we arrive at the upper limits on mass-loss rate for the progenitor system of SN 2013dy (2016coj, 2018gv, 2018pv, 2019np), to be less than 12 (2.8,1.3, 2.1, 1.7)EE(-8) solar masses per year (for a wind speed of 100 km/s). To SNe 2016coj, 2018gv, 2018pv and 2019np we add radio data for 17 other nearby SNe Ia, and model their non-detections. With the same model as described, all 21 SNe Ia have mass-loss rates less than 4EE(-8) solar masses per year (for a wind speed of 100 km/s). We compare those limits with the expected mass loss rates in different single-degenerate progenitor scenarios. We also discuss how information on epsilon_e and epsilon_B can be obtained from late observations of SNe Ia and the youngest SN Ia remnant detected in radio, G1.9+0.3, as well as stripped-envelope core-collapse SNe. We highlight SN 2011dh, and argue for epsilon_e approximately equal to 0.1 and epsilon_B approximately equal to 0.0033. Finally, we discuss strategies to observe at radio frequencies to maximize the chance of detection, given the time since explosion, the distance to the supernova and the telescope sensitivity.
