论文标题
将红外表面亮度波动距离连接到IA类型超新星宿主：测试距离梯子的顶部梯级
Connecting Infrared Surface Brightness Fluctuation Distances to Type Ia Supernova Hosts: Testing the Top Rung of the Distance Ladder
论文作者
论文摘要
我们比较了在托管IA型超新星（SNIA）的星系中测得的红外表面亮度波动（IR SBF）与从SNIA光曲线拟合估计的距离。我们表明，在IR SBF宿主中发现的SNIA的性质与在Cepheid校准器中爆炸的SNIA的特性大不相同，因此，这是对使用超新星对哈勃常数（HO）进行系统不确定性的直接测试。 IR SBF来自Jensen等人。 （2021; arxiv：2105.08299）提供了一个较大且均匀测量的IR SBF距离样品，我们将其与25个SNIA宿主星系进行了直接比较。我们将Hubble Flow SNIA分为子样本，这些子样本最能匹配IR SBF宿主和CepheID宿主中的不同超新星特性。我们将SNIA进一步分为具有光曲线宽度和宿主质量的样品，这些样品与在SBF校准的宿主中发现的样品相一致。我们将光曲线拉伸和亮度相关性与光度相关，并使用这些修订后的参数用IR SBF校准器校准了Hubble流量超新星。相对于哈勃流动，平均校准器距离模量根据所检查的SNIA子样本而变化0.03mag，这使我们的哈勃恒定估计值增加了1.8％的系统不确定性。基于IR SBF校准器，HO = 74.6 $ \ pm $ 0.9（stat）$ \ pm $ 2.7（SYST）km/s/mpc，这与从CepheID变量校准的超新星校准的哈勃常数一致。我们得出的结论是，IR SBF提供了可靠的SNIA校准，其精度可与头孢烷校准器相当，并且可以大量节省望远镜时间。
We compare infrared surface brightness fluctuation (IR SBF) distances measured in galaxies that have hosted type Ia supernovae (SNIa) to distances estimated from SNIa light curve fits. We show that the properties of SNIa found in IR SBF hosts are very different from those exploding in Cepheid calibrators, therefore, this is a direct test of systematic uncertainties on estimation of the Hubble constant (Ho) using supernovae. The IR SBF results from Jensen et al. (2021; arXiv:2105.08299) provide a large and uniformly measured sample of IR SBF distances which we directly compare with distances to 25 SNIa host galaxies. We divide the Hubble flow SNIa into sub-samples that best match the divergent supernova properties seen in the IR SBF hosts and Cepheid hosts. We further divide the SNIa into a sample with light curve widths and host masses that are congruent to those found in the SBF-calibrated hosts. We refit the light curve stretch and color correlations with luminosity, and use these revised parameters to calibrate the Hubble flow supernovae with IR SBF calibrators. Relative to the Hubble flow, the average calibrator distance moduli vary by 0.03mag depending on the SNIa subsamples examined and this adds a 1.8% systematic uncertainty to our Hubble constant estimate. Based on the IR SBF calibrators, Ho=74.6$\pm$0.9(stat)$\pm$ 2.7(syst) km/s/Mpc, which is consistent with the Hubble constant derived from supernovae calibrated from Cepheid variables. We conclude that IR SBF provides reliable calibration of SNIa with a precision comparable to Cepheid calibrators, and with a significant saving in telescope time.
