This Symposium was focused on the hunt for the progenitors of Supernovae of Type Ia. Is there a main channel for the production of SNeIa? If so, are these elusive progenitors Single Degenerate or Double Degenerate systems? Although most participants seemed to favour the Single Degenerate channel, there was no general agreement on the type of binary system at play. An observational puzzle that was highlighted was the apparent paucity of Super-Soft Sources in our Galaxy and also in external galaxies. The Single Degenerate channel (and as it was pointed out, quite possibly also the Double Degenerate channel) requires the binary system to pass through a phase of steady nuclear burning. However, the observed number of Super-Soft sources falls short by a factor of up to 100 in explaining the estimated birth rates of SNeIa. Thus, are these Super-Soft sources somehow hidden away and radiating at different wavelengths or are we missing some important pieces of this puzzle that may lead to the elimination of a certain class of progenitor? Another unanswered question concerns the dependence of SNeIa luminosities on the age of their host galaxy. Several hypotheses were put forward, but none was singled out as the most likely explanation.
It is fair to say that at the end of the Symposium the definitive answer to the vexed progenitor question remained is well and truly wide open.
Integral field spectroscopy of supernova explosion sites: constraining mass and metallicity of the progenitors -- II. Type II-P and II-L supernovae
利用积分场光谱学已经观测到了附近星系中II-P和II-L型超新星的13个爆炸点，使得对爆炸点的空间和光谱研究成为可能。我们利用同时代超新星祖先星的母恒星星族的性质来推导它的金属丰度和初始质量（c.f. Paper I）。母恒星星族的光谱通过强线方法得到金属丰度的估计，并通过与简单的恒星星族（SSP）模型的比较得到年龄。这些金属丰度和年龄参数被采用的祖星。通过与恒星演化模型的比较，利用恒星的年龄或寿命来推导恒星的初始质量。利用这种技术，我们能够确定我们样品中SN祖细胞的金属丰度和初始质量。我们的结果表明，一些II型超新星的祖先可能是质量与SN Ib/c祖先相当的恒星。
Type II Supernovae: Model Light Curves and Standard Candle Relationships
II型超新星爆炸模型的调查已经进行，以确定它们的光变曲线和光谱如何随它们的质量，金属丰度和爆炸能量而变化。前超新星模型取自最近对太阳金属丰度下大质量恒星演化的调查，并辅以太阳下金属丰度的新计算。爆炸是由一个活塞附近的铁芯的边缘的运动模拟和由此产生的光变曲线和光谱计算使用全多波长辐射输运。公式的开发，描述了大约如何模型观测（光变曲线光度和持续时间）规模与祖质量，爆炸能量，和放射性核合成。与观测数据的比较表明，典型超新星的爆炸能量（用无穷远处的动能来衡量）相差近一个数量级--从0.5到4.0 x 10^51尔格，典型值约为0.9 x 10^51尔格。尽管有很大的变化，模型表现出紧密的光度和膨胀速度之间的关系，类似于以前采用的经验，使SNe IIP标准化蜡烛。这种关系可以用超新星包层中氢复合的简单行为来解释，但是我们发现对祖先金属丰度和质量的敏感性可能导致系统误差。光变曲线光度、持续时间和颜色之间的其他相关性可能使SNe IIP能够仅使用光度数据获得精确到约20%的距离。
Observations of SN 2015F suggest a correlation between the intrinsic luminosity of Type Ia supernovae and the shape of their light curves >900 days after explosion
