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>The Type I Superluminous Supernova PS16aqv: Lightcurve Complexity and Deep Limits on Radioactive Ejecta in a Fast Event
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The Type I Superluminous Supernova PS16aqv: Lightcurve Complexity and Deep Limits on Radioactive Ejecta in a Fast Event
We present UV/optical observations of PS16aqv (SN 2016ard), a fast-evolving Type I superluminous supernova (SLSN-I) that reached a peak absolute magnitude of M r ?≈??22.1. The lightcurves exhibit a significant undulation at 30 rest-frame days after peak, with a behavior similar to undulations seen in the slowly fading SLSN-I SN 2015bn. This similarity strengthens the case that fast and slow SLSNe-I form a continuum with a common origin. At ≈80 days after peak, the lightcurves exhibit a transition to a slow decline, followed by significant steepening, indicative of a plateau phase or a second significant undulation. Deep limits at ≈280 days after peak imply a tight constraint on the nickel mass, M Ni??0.35 M ⊙ (lower than for previous SLSNe-I), and indicate that some SLSNe-I do not produce significantly more nickel than normal Type Ic SNe. Using MOSFiT, we model the lightcurve with a magnetar central engine model and find P spin?≈?0.9 ms, B?≈?1.5?×?1014 G, and M ej?≈?16 M ⊙. The implied rapid spin-down time and large reservoir of available energy coupled with the high ejecta mass may account for the fast lightcurve and slow spectroscopic evolution. We also study PS16aqv's location within its host galaxy and find that it occurred at an offset of 2.46?±?0.21 kpc from the central star-forming region. Aside from high extinction, the host properties are similar to most other SLSN-I host galaxies. The complexity in the lightcurves of PS16aqv and other events highlights the importance of obtaining well-sampled lightcurves for exploring deviations from a uniform decline.
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机译：我们提供PS16aqv（SN 2016ard）的紫外/光学观察结果，PS16aqv是一种快速发展的I型超发光超新星（SLSN-I），其峰值绝对强度为Mr≈≈22.1。峰值后30个静止帧天，光曲线显示出明显的起伏，其行为类似于在缓慢褪色的SLSN-I SN 2015bn中看到的起伏。这种相似性增强了快速和慢速SLSNe-I形成具有共同起源的连续体的情况。在峰值后约80天，光曲线呈现出向缓慢下降的过渡，随后出现明显的陡峭变化，表明出现了平稳阶段或第二次明显起伏。峰值后约280天的深限意味着对镍质量的严格限制，M Ni ?? 0.35 M⊙（低于以前的SLSNe-I），表明某些SLSNe-I不会比正常类型产生更多的镍。 Ic SNe。使用MOSFiT，我们用磁心中央引擎模型对光曲线进行建模，并找到Pspin≈≈0.9ms，B≈≈1.5××1014 G和Mej≈≈16M⊙。隐含的快速降速时间和大量可用能量，再加上高的喷射质量，可能是快速的光曲线和缓慢的光谱演化的原因。我们还研究了PS16aqv在其宿主星系中的位置，发现它发生在距中心恒星形成区域2.46？±？0.21 kpc的偏移处。除了高度消光外，宿主的属性与大多数其他SLSN-1宿主星系相似。 PS16aqv的光曲线和其他事件的复杂性凸显了获得良好采样的光曲线对于探索均匀下降偏差的重要性。
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