发表机构
Heidelberg Institute for Theoretical Studies; Max-Planck-Institut für Astrophysik; Lawrence Berkeley National Laboratory; Laboratoire de Physique Nucléaire et des Hautes Energies, CNRS/IN2P3, Sorbonne Université, Université de Paris; Yale University; European Space Astronomy Center (ESAC), European Space Agency; Univ Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon; European Southern Observatory（海德堡理论研究所; 马克斯·普朗克天体物理研究所; 劳伦斯伯克利国家实验室; 核物理与高能物理实验室，法国国家科学研究中心/法国国家原子能和替代能源委员会，索邦大学，巴黎大学; 耶鲁大学; 欧洲空间天文中心，欧洲航天局; 里昂大学，克莱贝尔·贝尔纳里昂第一大学，法国国家科学研究中心/法国国家原子能和替代能源委员会，里昂粒子物理研究所; 欧洲南方天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出基于分层贝叶斯和Hα吸收发射比修正的II-P型超新星标准化框架，将哈勃流离散度从0.28等降至0.18等，并测得H0=70.6 km/s/Mpc，精度6.2%。
AI 中文摘要
我们利用邻近超新星工厂（SNfactory）实验观测到的II-P型超新星（SNe II-P）作为标准烛光，开发了一种改进的标准化框架。数据包括低红移SNe II-P在波长范围$3200 < \lambda < 10000$ ${\unicode{xC5}}$内的精确流量定标、宿主星系扣除的光谱光度测量。我们开发了一种基于高斯过程回归的改进方法来确定SNe II-P的膨胀速度。我们通过包含H$\alpha$吸收与发射比率的额外修正项和分层贝叶斯框架扩展了传统的标准烛光方法（SCM）。我们发现，额外的修正提高了标准化的质量，特别是在爆炸后约30至40天。与先前工作相比，我们能够将哈勃流SNe II-P的离散度从0.28等降低到0.18等。作为该方法的一个应用示例，我们使用预先存在的、具有造父变星或TRGB距离模数的SNe II校准样本测量了$H_0$。我们发现$H_0 = 70.6^{+4.5}_{-4.3}$ km s$^{-1}$ Mpc$^{-1}$，仅包括统计不确定性，对应精度为6.2%。我们发现分层模型变体之间的变化为1.4 km s$^{-1}$ Mpc$^{-1}$——远在我们引用的统计不确定性范围内。如果没有额外的修正项，我们得到$H_0 = 73.0^{+6.9}_{-6.1}$ km s$^{-1}$ Mpc$^{-1}$（8.9%精度），突显了我们新方法的改进精度。我们识别并讨论了校准器和哈勃流标准化特征之间测量的母体种群的不一致性——这些存在于本文和文献样本中——这些不一致性无法通过简单的星等选择来解释，并且随着SN II-P样本的增长需要改进。
英文摘要
We use Type II-P supernovae (SNe II-P) observed as part of the Nearby Supernova Factory (SNfactory) experiment as standardizable candles to develop an improved standardization framework. The data consist of accurately flux-calibrated, host-subtracted spectrophotometry of low-redshift SNe II-P in the wavelength range $3200 < λ< 10000$ ${\unicode{xC5}}$. We develop an improved method to determine the expansion velocities of SNe II-P based on Gaussian Process regression. We extend the conventional standardized candle method (SCM) by an additional correction term containing the H$_α$ absorption-to-emission ratio and a hierarchical Bayesian framework. We find that the additional correction improves the quality of the standardization, particularly around $30$ to $40$ days after the explosion. We are able to reduce the scatter of the Hubble-flow SNe II-P from $0.28$ mag down to $0.18$ mag compared to previous work. As an example application of this methodology we measure $H_0$ using a pre-existing calibrator sample of SNe~II having Cepheid- or TRGB-based distance moduli. We find a value of $H_0 = 70.6^{+4.5}_{-4.3}$ km s$^{-1}$ Mpc$^{-1}$, including only statistical uncertainty, corresponding to a precision of $6.2$%. We find variations of $1.4$ km s$^{-1}$ Mpc$^{-1}$ between hierarchical model variations --- well within our quoted statistical uncertainty. Without the additional correction term, we obtain $H_0 = 73.0^{+6.9}_{-6.1}$ km s$^{-1}$ Mpc$^{-1}$ ($8.9$% precision) highlighting the improved precision of our new methodology. We identify and discuss inconsistencies between the measured parent populations of the calibrator and Hubble-flow standardization characteristics --- present in this and literature samples --- that are not explained by a simple selection on magnitude and which will need to be improved upon as SN II-P samples grow.
Comments54 pages, 67 figures, accepted for publication in A&A. Appendices contain additional figures compared to the A&A version
