The snapshot distance method：从最小观测估计Ia型超新星的距离
The snapshot distance method: estimating the distance to a Type Ia supernova from minimal observations
摘要：
我们提出的快照距离方法（SDM），一个现代的化身，提出的技术估计距离Ia型超新星（SN Ia）从最小的观测。由于最近将深度学习应用于SN Ia光谱的工作（我们使用deepSIP包），我们的方法已经成为可能，使我们能够从单个光谱和$2+$通带测光的历元中估计到SN Ia的距离-一个晚上的观测值（尽管同期性不是必需的）。使用汇编观测良好的超新星Ia，我们产生快照的距离在很宽的范围内的光谱和光度相位，光曲线形状，光度通带组合，和光谱信噪比。通过将这些估计与每个对象的所有可用测光拟合得到的相应距离进行比较，我们证明了我们的方法对所提供的光谱和光度信息的相对时间采样具有鲁棒性，并且对位于标准宽度-光度关系域内的广泛的光曲线形状具有鲁棒性。事实上，中值残差（和不对称散射）SDM距离来自两个通带测光和传统的光变曲线推导的距离，利用所有可用的测光是$0.013_{-0.143}^{+0.154}$马格。此外，我们发现，最大亮度和光变曲线形状的时间（这两个都是光谱在我们的方法得出的）只最低限度地负责所观察到的散射。在一个配套文件中，我们将SDM应用到大量的稀疏观测的超新星Ia作为宇宙学研究的一部分。
英文摘要：
We present the snapshot distance method (SDM), a modern incarnation of a proposed technique for estimating the distance to a Type Ia supernova (SN Ia) from minimal observations. Our method, which has become possible owing to recent work in the application of deep learning to SN Ia spectra (we use the deepSIP package), allows us to estimate the distance to an SN Ia from a single optical spectrum and epoch of $2+$ passband photometry -- one night's worth of observations (though contemporaneity is not a requirement). Using a compilation of well-observed SNe Ia, we generate snapshot distances across a wide range of spectral and photometric phases, light-curve shapes, photometric passband combinations, and spectrum signal-to-noise ratios. By comparing these estimates to the corresponding distances derived from fitting all available photometry for each object, we demonstrate that our method is robust to the relative temporal sampling of the provided spectroscopic and photometric information, and to a broad range of light-curve shapes that lie within the domain of standard width-luminosity relations. Indeed, the median residual (and asymmetric scatter) between SDM distances derived from two-passband photometry and conventional light-curve-derived distances that utilise all available photometry is $0.013_{-0.143}^{+0.154}$ mag. Moreover, we find that the time of maximum brightness and light-curve shape (both of which are spectroscopically derived in our method) are only minimally responsible for the observed scatter. In a companion paper, we apply the SDM to a large number of sparsely observed SNe Ia as part of a cosmological study.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
