The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations
The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations
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AMI 无线电观测揭示了 SN 2014C 奇特的质量损失历史
DOI：
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
D. Titterington
中科院分区：
文献类型：
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作者：
G. Anderson;G. Anderson;A. Horesh;A. Horesh;K. Mooley;A. Rushton;A. Rushton;R. Fender;T. Staley;M. Argo;M. Argo;R. Beswick;P. Hancock;P. Hancock;M. Pérez;M. Pérez;Y. Perrott;R. Plotkin;M. Pretorius;C. Rumsey;D. Titterington
我们展示了使用Arcminute Microkelvin Imager（AMI）大型阵列在15.7 GHz下拍摄的超新星（SN）2014 C的射电光曲线。Milisavljevic等人的光学观测表明，SN 2014 C在1年内从一个剥层的Ib型SN蜕变为一个强相互作用的IIn型SN。AMI光变曲线清楚地显示出两种不同的
无线电峰值，第二个是比第一个峰值更明亮的4倍的因子。这种双凸起的形态表明，两个不同的阶段，从祖星星的质量损失与密度之间的过渡制度发生在100-200 d。这加强了SN 2014 C在低密度区域爆炸的解释，然后遇到了一个致密的富含氢的壳层，该壳层可能是在爆炸前由祖先喷射出来的。
第一个光变曲线凸起的AMI通量测量是爆炸后2050至20125天内，在冲击波遇到氢壳层之前进行的唯一报告观测。简单的同步加速器自吸收和自由-自由吸收模型表明，SN 2014 C的一些物理性质与其他Ibc型的性质一致
我在SNE。然而，我们的单频数据不允许我们区分这两种模型，这意味着它们可能过于简单，无法描述围绕这一事件的复杂环境。最后，我们提出了精确的无线电定位SN 2014 C获得的电子多元远程链接干涉仪网络，这将是有用的，为未来的SN的甚长基线干涉测量观测。
We present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped-envelope Type Ib SN into a strongly interacting Type IIn SN within 1 yr. The AMI light curve clearly shows two distinct
radio peaks, the second being a factor of 4 times more luminous than the first peak. This double bump morphology indicates two distinct phases of mass-loss from the progenitor star with the transition between density regimes occurring at 100–200 d. This reinforces the interpretation that SN 2014C exploded in a low-density region before encountering a dense hydrogen-rich shell of circumstellar material that was likely ejected by the progenitor prior to the explosion.
The AMI flux measurements of the first light-curve bump are the only reported observations taken within ∼50 to ∼125 d post-explosion, before the blast-wave encountered the hydrogen shell. Simplistic synchrotron self-absorption and free–free absorption modelling suggest that some physical properties of SN 2014C are consistent with the properties of other Type Ibc
and IIn SNe. However, our single frequency data does not allow us to distinguish between these two models, which implies that they are likely too simplistic to describe the complex environment surrounding this event. Lastly, we present the precise radio location of SN 2014C obtained with the electronic Multi-Element Remotely Linked Interferometer Network, which will be useful for future very long baseline interferometry observations of the SN.
影响因子：
4.8
作者：
G. Anderson;A. Horst;T. Staley;R. Fender;R. Wijers;A. Scaife;C. Rumsey;D. Titterington;A. Rowlinson;R. D. E. S. U. Southampton;U. Oxford;U. Amsterdam;U. Cambridge
通讯作者：
G. Anderson;A. Horst;T. Staley;R. Fender;R. Wijers;A. Scaife;C. Rumsey;D. Titterington;A. Rowlinson;R. D. E. S. U. Southampton;U. Oxford;U. Amsterdam;U. Cambridge