M82中Ia型SN 2014 J的前4个月中红外光谱
Mid-IR Spectra of Type Ia SN 2014J in M82 Spanning the First Four Months
摘要：
我们提出了一个时间序列的8 - 13 $μ$ m光谱和测光SN 2014 J获得57，81，108，和137天后，使用大加那利望远镜上的CanariCam爆炸。这是有史以来第一次获得Ia型超新星的中红外时间序列。这些观察结果可以在延迟爆轰模型和$^{56}$ Ni的$\sim$ 0.6 $\rm M_\odot$的产生的框架内理解，与观察到的亮度、亮度下降关系和$γ$射线通量一致。在11.888 $μ$ m处的[Co III]线对于评估光球的时间演化和测量$^{56}$ Ni的量以及由此测量喷出物的质量特别有用。SN 2014 J的晚期谱线轮廓相当对称，在静止帧中没有偏移。我们看到了氩的发射，它提供了一个独特的探测混合在过渡层之间的不完全燃烧和核统计平衡。我们可能会看到[Fe III]和[Ni IV]的发射，这两种发射都比我们的模型显示的要强得多。如果后一种识别是正确的，那么我们可能会观察到稳定的Ni，这可能意味着中心混合。此外，稳定的镍也需要电子捕获，需要密度大于$\sim$ $1 \times 10^9$ g cm $^{-3}$，这预计只存在于接近于克拉塞卡极限的白矮星中。这项研究表明，从地面对Ia型超新星进行中红外研究是可行的，并提供了独特的信息，但它也表明需要更好的原子数据。
英文摘要：
We present a time series of 8 - 13 $μ$m spectra and photometry for SN 2014J obtained 57, 81, 108, and 137 d after the explosion using CanariCam on the Gran Telescopio Canarias. This is the first mid-IR time series ever obtained for a Type Ia supernova. These observations can be understood within the framework of the delayed detonation model and the production of $\sim$0.6 $\rm M_\odot$ of $^{56}$Ni, consistent with the observed brightness, the brightness decline relation, and the $γ$-ray fluxes. The [Co III] line at 11.888 $μ$m is particularly useful for evaluating the time evolution of the photosphere and measuring the amount of $^{56}$Ni and thus the mass of the ejecta. Late-time line profiles of SN 2014J are rather symmetric and not shifted in the rest frame. We see Argon emission, which provides a unique probe of mixing in the transition layer between incomplete burning and nuclear statistical equilibrium. We may see [Fe III] and [Ni IV] emission, both of which are observed to be substantially stronger than indicated by our models. If the latter identification is correct, then we are likely observing stable Ni, which might imply central mixing. In addition, electron capture, also required for stable Ni, requires densities larger than $\sim$$1 \times 10^9$ g cm$^{-3}$, which are expected to be present only in white dwarfs close to the Chandrasekhar limit. This study demonstrates that mid-IR studies of Type Ia supernovae are feasible from the ground and provide unique information, but it also indicates the need for better atomic data.
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