A Bright Ultraviolet Excess in the Transitional 02es-like Type Ia Supernova 2019yvq-猫眼课题宝

DOI：

10.3847/1538-4357/ac126b

发表时间：

2021-01

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

J. Burke;D. Howell;S. Sarbadhicary;D. Sand;R. Amaro;D. Hiramatsu;C. McCully;C. Pellegrino;J. Andrews;P. Brown;Koichi 公一 Itagaki 板垣;M. Shahbandeh;K. Bostroem;L. Chomiuk;E. Hsiao;N. Smith;S. Valenti

我们介绍了附近Ia型SN 2019yvq的光度和光谱观测，从爆炸后约1天到其峰值亮度后约100天。这颗超新星表现出几个不寻常的特征，最明显的是在爆炸后5天内出现了非常明亮的紫外线过量。从Swift的紫外线数据中可以看到，这种早期的过量超过了它的“峰值”亮度，使得这个天体比其他具有早期紫外线/蓝色过量的超新星（例如iPTF14atg和SN 2017cbv）更加极端。此外，它是弱光的M B =−18.4，相对迅速地下降（Δm 15(B) = 1.37），并在早期的蓝色凸起后呈现红色。不寻常的（虽然不是前所未有的）光谱特征包括极宽的线和高速硅吸收。尽管SN 2019yvq的峰值光谱存在明显差异，但由于其在颜色、峰值光度、峰值Ti和星云[Ca ii]等方面的相似性，我们将其归类为类02s亚类的过渡成员。我们使用各种已发表的模型对该数据集进行建模，包括SN抛射-伴随激波相互作用和次钱德拉塞卡-质量白矮星（WD）双爆模型。来自VLA的射电约束给出了共生前身质量损失率的上限（4.5-20）× 10−8 M⊙yr−1，这并不排除红巨星或主序伴星。最终，我们发现没有一个模型可以准确地复制数据集的所有方面，并且我们进一步发现，像超新星Ia这样的02年早期过度的普遍存在需要一个能够产生各向同性紫外线通量的祖系统，从而排除了这类物体的一些模型。

We present photometric and spectroscopic observations of the nearby Type Ia SN 2019yvq, from its discovery ∼1 day after explosion to ∼100 days after its peak brightness. This SN exhibits several unusual features, most notably an extremely bright UV excess seen within ∼5 days of its explosion. As seen in Swift UV data, this early excess outshines its “peak” brightness, making this object more extreme than other supernovae (SNe) with early UV/blue excesses (e.g., iPTF14atg and SN 2017cbv). In addition, it was underluminous M B = −18.4, relatively quickly declining (Δm 15(B) = 1.37), and shows red colors past its early blue bump. Unusual (although not unprecedented) spectral features include extremely broad-lined and high-velocity Si absorption. Despite obvious differences in peak spectra, we classify SN 2019yvq as a transitional member of the 02es-like subclass due to its similarities in several respects (e.g., color, peak luminosity, peak Ti, and nebular [Ca ii]). We model this data set with a variety of published models, including SN ejecta–companion shock interaction and sub-Chandrasekhar-mass white dwarf (WD) double-detonation models. Radio constraints from the VLA place an upper limit of (4.5–20) × 10−8 M ⊙ yr−1 on the mass-loss rate from a symbiotic progenitor, which does not exclude a red giant or main-sequence companion. Ultimately, we find that no one model can accurately replicate all aspects of the data set, and further we find that the ubiquity of early excesses in 02es-like SNe Ia requires a progenitor system that is capable of producing isotropic UV flux, ruling out some models for this class of objects.

A Bright Ultraviolet Excess in the Transitional 02es-like Type Ia Supernova 2019yvq

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