I型超亮超新星2020znr的后极大光和晚时光学成像偏振测量
Post maximum light and late time optical imaging polarimetry of type I superluminous supernova 2020znr
摘要：
光学成像偏振测量是在贫氢超亮超新星2020znr最大光照后的3个阶段（大约+34天，+288天和+289天）进行的。经过仪器和星际偏振校正，所有测量结果与零偏振探测一致。用磁星自旋下降模型模拟的光变曲线表明SN 2020znr与其他SLSNe具有相似的磁星和喷出物参数。在SN 2017egm和SN 2015bn的文献中讨论的最佳拟合值的比较，两个贫氢SLSNe显示最大光后的偏振增加，表明SN 2020znr具有更高质量的喷出物，可能会阻止使用光学偏振测量的内部喷出物的几何形状。I型SLSNe的光谱学和光变曲线分析提供的组合信息可能是对这类瞬态的偏振特性进行分类的一个有趣途径。这种方法将需要扩大SLSNe偏振测量数据的样本，目前可与早期和晚期的时间新的测量。
英文摘要：
Optical imaging polarimetry was conducted on the hydrogen poor superluminous supernova 2020znr during 3 phases after maximum light (approximately +34 days, +288 days and +289 days). After instrumental and interstellar polarization correction, all measurements are consistent with null-polarization detection. Modelling the light curve with a magnetar spin-down model shows that SN 2020znr has similar magnetar and ejecta parameters to other SLSNe. A comparison of the best-fit values discussed in the literature on SN 2017egm and SN 2015bn, two hydrogen poor SLSNe showing an increase of polarization after maximum light, suggests that SN 2020znr has higher mass ejecta that may prevent access to the geometry of the inner ejecta with optical polarimetry. The combined information provided by spectroscopy and light curve analysis of type I SLSNe may be an interesting avenue to categorize the polarization properties of this class of transients. This approach would require to expand the sample of SLSNe polarimetry data currently available with early and late time epochs new measurements.
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