The Deepest Radio Observations of Nearby SNe Ia: Constraining Progenitor Types and Optimizing Future Surveys
The Deepest Radio Observations of Nearby SNe Ia: Constraining Progenitor Types and Optimizing Future Surveys
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DOI：
10.3847/1538-4357/ab6dc6
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发表时间：
2020-01
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通讯作者：
P. Lundqvist;E. Kundu;M. Pérez-Torres;S. Ryder;C. Björnsson;J. Moldón;M. Argo;R. Beswick;A. Alberdi;E. Kool
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作者：
P. Lundqvist;E. Kundu;M. Pérez-Torres;S. Ryder;C. Björnsson;J. Moldón;M. Argo;R. Beswick;A. Alberdi;E. Kool
我们报告了用电子多元素无线电连接干涉仪网络和澳大利亚望远镜紧凑阵列对附近Ia型超新星（SNe Ia）的深射电观测。没有进行检测。根据相对论电子能量密度进入幂律能量分布和磁场强度（ϵe = ϵB = 0.1）的标准假设，我们得到了SN 2013dy祖系统（SN 2016coj, SN 2018gv, SN 2018pv, SN 2019np）的质量损失率上限，其中vw为质量损失的风速。对于SN 2016coj、SN 2018gv、SN 2018pv和SN 2019np，我们添加了附近其他17个SN Ia的无线电数据，并对它们的未检测进行了建模。与描述的模型相同，所有21个sni都有。我们将这些极限与不同单简并前体情景下的期望质量损失率进行了比较。我们还讨论了如何从Ia超新星和射电中发现的最年轻的Ia超新星遗迹G1.9+0.3以及剥离包络核坍缩SNe的后期观测中获得ϵe和ϵB的信息。我们强调SN 2011dh，并认为ϵe≈0.1和ϵB≈0.0033。最后，我们讨论了在给定爆炸时间、到超新星的距离和望远镜灵敏度的情况下，在无线电频率上观测以最大限度地提高探测机会的策略。
We report deep radio observations of nearby Type Ia supernovae (SNe Ia) with the electronic Multi-Element Radio Linked Interferometer Network and the Australia Telescope Compact Array. 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 (ϵe = ϵB = 0.1), we arrive at upper limits on mass-loss rate for the progenitor system of SN 2013dy (SN 2016coj, SN 2018gv, SN 2018pv, SN 2019np) of , where vw is the wind speed of the mass loss. To SN 2016coj, SN 2018gv, SN 2018pv, and SN 2019np we add radio data for 17 other nearby SNe Ia and model their nondetections. With the same model as described, all 21 SNe Ia have . We compare those limits with the expected mass-loss rates in different single-degenerate progenitor scenarios. We also discuss how information on ϵe and ϵB 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 ϵe ≈ 0.1 and ϵB ≈ 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 SN, and the telescope sensitivity.