Evidence for a Pulsar Wind Nebula in the Type Ib Peculiar Supernova SN 2012au
Evidence for a Pulsar Wind Nebula in the Type Ib Peculiar Supernova SN 2012au
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DOI：
10.3847/2041-8213/aadd4e
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发表时间：
2018-09
期刊：
影响因子：
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通讯作者：
D. Milisavljevic;D. Patnaude;R. Chevalier;J. Raymond;R. Fesen;R. Margutti;Brody Conner;J. Banovetz
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文献类型：
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作者：
D. Milisavljevic;D. Patnaude;R. Chevalier;J. Raymond;R. Fesen;R. Margutti;Brody Conner;J. Banovetz
我们展示了在爆炸后 6.2 年史无前例的时期获得的高能 Ib 型超新星 (SN) 2012au 的光谱。氧和硫的禁止跃迁发射线以约 2300 km s−1 的膨胀速度被检测到。窄 H 巴尔默线的缺乏表明，与星周物质的相互作用并不是观测到的后期发射的主要来源。我们还提出了深度钱德拉观测，表明在 LX < 2 × 1038 erg s−1 (0.5–10 keV) 的光度下没有 X 射线发射。我们的研究结果与SN 2012au与超新星的不同子集有关的观点是一致的，包括长持续时间伽马射线暴超新星和超光度超新星，它们蕴藏着脉冲星/磁风星云，在广泛的能量尺度上影响核心塌缩爆炸动力学。我们假设这些系统可能都演变成一个类似的由禁止氧跃迁主导的后期阶段，并预测由于脉冲星/磁气泡加速喷射物，发射线宽度应保持恒定或每年加宽几个百分点。
We present an optical spectrum of the energetic Type Ib supernova (SN) 2012au obtained at an unprecedented epoch of 6.2 yr after explosion. Forbidden transition emission lines of oxygen and sulfur are detected with expansion velocities of ≈2300 km s−1. The lack of narrow H Balmer lines suggests that interaction with circumstellar material is not a dominant source of the observed late-time emission. We also present a deep Chandra observation that reveals no X-ray emission down to a luminosity of LX < 2 × 1038 erg s−1 (0.5–10 keV). Our findings are consistent with the notion that SN 2012au is associated with a diverse subset of SNe, including long-duration gamma-ray burst SNe and superluminous SNe, harboring pulsar/magnetar wind nebulae that influence core-collapse explosion dynamics on a wide range of energy scales. We hypothesize that these systems may all evolve into a similar late-time phase dominated by forbidden oxygen transitions, and predict that emission line widths should remain constant or broaden a few percent per year due to the acceleration of ejecta by the pulsar/magnetar bubble.