论文标题
Galex-PTF实验：II。超新星祖细胞半径和通过冲击冷却建模
The GALEX-PTF experiment: II. supernova progenitor radius and energetics via shock-cooling modeling
论文作者
论文摘要
可以使用早期的紫外线（UV）观察结果测量爆炸巨星的半径和表面组成以及每单位质量的爆炸能量。我们介绍了同时\ Galex和Palomar Transient Factory（PTF）搜索SNE早期紫外线排放的结果。我们分析了五个CC SNE，在第一个基于地面的$ r $ band检测之前，我们为此获得了$ nuv $的测量。我们介绍了Sopranos，这是一种用于具有可变时间有效性窗口的模型的新型最大似然拟合工具，并将其用于将\ citet {sapirwaxman2017}减震冷却模型适合数据。我们在$ r _*\大约600-1100r_ \ odot $和一个冲击速度参数的范围内报告四型II类SNE，范围为$ v_ {s*} \ 2700-6000 \ \，\ rm km km km km km km \，s^{ - 1} $（$ e/m \ oftimm） erg/M_\odot$) and one type IIb SN with $R_*\approx210R_\odot$ and $v_{s*}\approx11000 \rm\, km\,s^{-1}$ ($E/M\approx1.8\times10^{51}\,\rm erg/M_\odot$).因此，我们的飞行员Galex/PTF项目表明，在$ nuv $ band中进行专门的，系统的SN调查，例如宽阔的紫外线Explorer \ textit {ultrasat} Mission，是研究SN祖细胞和SN Energetics的特性的引人入胜的方法。
The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early ultraviolet (UV) observations of core-collapse supernovae (CC SNe). We present the results from a simultaneous \GALEX and Palomar Transient Factory (PTF) search for early UV emission from SNe. We analyze five CC SNe for which we obtained $NUV$ measurements before the first ground-based $R$-band detection. We introduce SOPRANOS, a new maximum likelihood fitting tool for models with variable temporal validity windows, and use it to fit the \citet{SapirWaxman2017} shock cooling model to the data. We report four Type II SNe with progenitor radii in the range of $R_*\approx600-1100R_\odot$ and a shock velocity parameter in the range of $v_{s*}\approx 2700-6000 \,\rm km\,s^{-1}$ ($E/M\approx2-8\times10^{50}\,\rm erg/M_\odot$) and one type IIb SN with $R_*\approx210R_\odot$ and $v_{s*}\approx11000 \rm\, km\,s^{-1}$ ($E/M\approx1.8\times10^{51}\,\rm erg/M_\odot$). Our pilot GALEX/PTF project thus suggests that a dedicated, systematic SN survey in the $NUV$ band, such as the wide-field UV explorer \textit{ULTRASAT} mission, is a compelling method to study the properties of SN progenitors and SN energetics.
