论文标题
限制SN IA主机Galaxy Dust Law Law分布和质量步骤：光学和近红外光曲线的分层贝叶斯分析
Constraining the SN Ia Host Galaxy Dust Law Distribution and Mass Step: Hierarchical BayeSN Analysis of Optical and Near-Infrared Light Curves
论文作者
论文摘要
We use the BayeSN hierarchical probabilistic SED model to analyse the optical-NIR ($BVriYJH$) light curves of 86 Type Ia supernovae (SNe Ia) from the Carnegie Supernova Project to investigate the SN Ia host galaxy dust law distribution and correlations between SN Ia Hubble residuals and host mass.我们的贝叶斯分析同时通过利用光学NIR颜色信息来限制质量步骤和灰尘$ r_v $种群分布。我们演示了如何单独估算每个SN的单个$ r_v $值的简单分析，然后计算这些点估计的样本差异，高估了$ r_v $ superity差异$σ_r^2 $。当由于光曲线形状而忽略了残留的固有颜色变化时，这种偏见会加剧。取而代之的是，贝叶斯的收缩估计值为$σ_r$更准确，对光曲线的完全分层分析是理想的。对于具有低至中度红色的75 SNE（峰值$ b-v \ leq0.3 $），我们估计$ r_v $分布的人口平均$μ_r= 2.59 \ pm0.14 $和标准偏差$σ_R= 0.62 \ pm0.16 $。将此子样本在中位主机星系质量（$ 10^{10.57}〜\ Mathrm {M} _ \ odot $）中产生一致的估计估计的低质量星系和高质量星系之间的$ r_v $分布，$μ_r= 2.79 $μ_r= 2.35 \ pm0.27 $，$σ_r= 0.74 \ pm0.36 $。当估计距整个光学光曲线的距离，同时在各种形式的灰尘$ r_v $分布上进行边缘化时，质量步骤为$ \ gtrsim0.06 $ mag在中位宿主质量的哈勃残留物中仍然存在。
We use the BayeSN hierarchical probabilistic SED model to analyse the optical-NIR ($BVriYJH$) light curves of 86 Type Ia supernovae (SNe Ia) from the Carnegie Supernova Project to investigate the SN Ia host galaxy dust law distribution and correlations between SN Ia Hubble residuals and host mass. Our Bayesian analysis simultaneously constrains the mass step and dust $R_V$ population distribution by leveraging optical-NIR colour information. We demonstrate how a simplistic analysis where individual $R_V$ values are first estimated for each SN separately, and then the sample variance of these point estimates is computed, overestimates the $R_V$ population variance $σ_R^2$. This bias is exacerbated when neglecting residual intrinsic colour variation beyond that due to light curve shape. Instead, Bayesian shrinkage estimates of $σ_R$ are more accurate, with fully hierarchical analysis of the light curves being ideal. For the 75 SNe with low-to-moderate reddening (peak apparent $B-V\leq0.3$), we estimate an $R_V$ distribution with population mean $μ_R=2.59\pm0.14$, and standard deviation $σ_R=0.62\pm0.16$. Splitting this subsample at the median host galaxy mass ($10^{10.57}~\mathrm{M}_\odot$) yields consistent estimated $R_V$ distributions between low- and high-mass galaxies, with $μ_R=2.79\pm0.18$, $σ_R=0.42\pm0.24$, and $μ_R=2.35\pm0.27$, $σ_R=0.74\pm0.36$, respectively. When estimating distances from the full optical-NIR light curves while marginalising over various forms of the dust $R_V$ distribution, a mass step of $\gtrsim0.06$ mag persists in the Hubble residuals at the median host mass.
