SN 2011fe是一代人中距离最近、观测最好的Ia型超新星，它使以前不完整的数据集与详细的新数据形成鲜明对比。回顾过去，记录Ia型超新星的光谱行为往往受到稀疏和不完整的时间采样的限制，而不是受到信噪比、大地特征或小样本大小的影响。因此，Ia型超新星的研究主要是通过相对时期和最大光附近的不完整时间快照离散化的参数。在这里，我们讨论了一致的建模和直接测量光谱观测的Ia型超新星光谱的必要的下一步。此外，我们分析了当前光谱数据的参数空间定义的经验指标，这将是相关的，即使在祖细胞被观察和详细的模型进行了改进。
英文摘要：
SN 2011fe was the nearest and best-observed type Ia supernova in a generation, and brought previous incomplete datasets into sharp contrast with the detailed new data. In retrospect, documenting spectroscopic behaviors of type Ia supernovae has been more often limited by sparse and incomplete temporal sampling than by consequences of signal-to-noise ratios, telluric features, or small sample sizes. As a result, type Ia supernovae have been primarily studied insofar as parameters discretized by relative epochs and incomplete temporal snapshots near maximum light. Here we discuss a necessary next step toward consistently modeling and directly measuring spectroscopic observables of type Ia supernova spectra. In addition, we analyze current spectroscopic data in the parameter space defined by empirical metrics, which will be relevant even after progenitors are observed and detailed models are refined.
International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research, Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；Center for Exotic Nuclear Studies, Institute for Basic Science（基础科学研究院）
Motivated by their role as the direct or indirect source of many of the elements in the Universe, numerical modeling of core collapse supernovae began more than five decades ago. Progress toward ascertaining the explosion mechanism(s) has been realized through increasingly sophisticated models, as physics and dimensionality have been added, as physics and numerical modeling have improved, and as the leading computational resources available to modelers have become far more capable. The past five to ten years have witnessed the emergence of a consensus across the core collapse supernova modelin…
This paper aims to give a brief review of a new concept for the preliminary determination of the evolutionary status of supernova remnants (SNRs). Data obtained by radio observations in continuum are used. There are three different methods underlying the new concept: the first one based on the location of observationally obtained radio surface brightness and corresponding diameter of an SNR on the theoretically derived Sigma-D tracks; the second one based on the forms of radio spectra; and the third one, based on the magnetic field strengths that are estimated through the equipartition (eqp) c…
We generate $\sim$ 100,000 model spectra of Type Ia Supernovae (SNIa) to form a spectral library for the purpose of building an Artificial Intelligence Assisted Inversion (AIAI) algorithm for theoretical models. As a first attempt, we restrict our studies to time around $B$-band maximum and compute theoretical spectra with a broad spectral wavelength coverage from 2000 $-$ 10000 ${\rm Å}$ using the code TARDIS. Based on the library of theoretically calculated spectra, we construct the AIAI algorithm with a Multi-Residual Convolutional Neural Network (MRNN) to retrieve the contributions of diff…
The Spectral SN-GRB Connection: Systematic Spectral Comparisons between Type Ic Supernovae, and broad-lined Type Ic Supernovae with and without Gamma-Ray Bursts
A quantitative data-driven comparison among supernovae (SNe) based on their spectral time series combined with multi-band photometry is presented. We use an unsupervised Random Forest algorithm as a metric on a set of 82 well-documented SNe representing all the main spectroscopic types, in order to embed these in an abstract metric space reflecting shared correlations between the objects. We visualize the resulting metric space in 3D, revealing strong agreement with the current spectroscopic classification scheme. The embedding splits Type Ib supernovae into two groups, with one subgroup exhib…
We present ultraviolet line identifications of near maximum-light HST observations of SN 2011fe using synthetic spectra generated from both SYNOW and $\texttt{PHOENIX}$. We find the spectrum to be dominated by blends of iron group elements Fe, Co, and Ni (as expected due to heavy line blanketing by these elements in the UV) and for the first time identify lines from C IV and Si IV in a supernova spectrum. We also find that classical delayed detonation models of Type Ia supernovae are able to accurately reproduce the flux levels of SN 2011fe in the UV. Further analysis reveals that photionizati…
