SN 2019 hcc：一颗II型超新星发现早期O型II线
SN 2019hcc: A Type II Supernova Displaying Early O II Lines
摘要：
我们提出的光谱学与紫外，光学和近红外测光SN 2019 hcc，它驻留在一个主机星系在红移0.044，显示太阳下的金属丰度。超新星光谱在4000埃附近呈现出一个“w”形，通常与O II线有关，是典型的I型超亮超新星。SN 2019 hcc的峰后光谱显示了一个从极大值过去19天开始的发展良好的H alpha P-Cygni轮廓，其光变曲线，就绝对峰值光度和演化而言，类似于快速下降的富氢超新星（SN IIL）。该物体没有显示出任何明确的相互作用迹象，因为没有证据表明光谱中存在窄线或光变曲线中存在波动。我们的tardis光谱建模的第一个光谱表明，碳，氮和氧（CNO）在19000 K复制的“W”形状，并建议在8000 K的非热激发的CNO和金属线的组合可以复制在4000 ℃看到的功能。测辐射热光变曲线模型显示SN 2019 hcc可以用磁星模型来拟合，显示出相对较强的磁场（B > 3 x 10^14 G），这与峰值亮度和上升时间相匹配，而无需将光变曲线提升到超亮亮度。磁星所产生的高能光子将是探测到的O II线的来源。因此，SN 2019 hcc显示，在4000光年左右的“w”形轮廓，通常归因于O II，不仅在超亮超新星中显示，因此它不应该被视为属于这种超新星类型的唯一证据。
英文摘要：
We present optical spectroscopy together with ultraviolet, optical and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a `w' shape at around 4000 Å which is usually associated with O II lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed H alpha P-Cygni profile from 19 days past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL). The object does not show any unambiguous sign of interaction as there is no evidence of narrow lines in the spectra or undulations in the light curve. Our tardis spectral modelling of the first spectrum shows that Carbon, Nitrogen and Oxygen (CNO) at 19000 K reproduce the `w' shape and suggests that a combination of non-thermally excited CNO and metal lines at 8000 K could reproduce the feature seen at 4000 Å. The Bolometric light curve modelling reveals that SN 2019hcc could be fit with a magnetar model, showing a relatively strong magnetic field (B > 3 x 10^14 G), which matches the peak luminosity and rise time without powering up the light curve to superluminous luminosities. The high-energy photons produced by the magnetar would then be responsible for the detected O II lines. As a consequence, SN 2019hcc shows that a `w' shape profile at around 4000 Å, usually attributed to O II, is not only shown in superluminous supernovae and hence it should not be treated as the sole evidence of the belonging to such a supernova type.
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