A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations
A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations
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DOI：
10.1051/0004-6361/202039196
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发表时间：
2020-08
影响因子：
6.5
通讯作者：
N. Khetan;L. Izzo;M. Branchesi;R. Wojtak;M. Cantiello;C. Murugeshan;A. Agnello;E. Cappellaro
中科院分区：
文献类型：
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作者：
N. Khetan;L. Izzo;M. Branchesi;R. Wojtak;M. Cantiello;C. Murugeshan;A. Agnello;E. Cappellaro
我们提出了一个新的校准的峰值绝对星等的Ia型超新星（SNe Ia）的基础上的表面亮度波动（SBF）的方法，旨在测量哈勃常数的值。我们建立了一个样本的校准锚组成的24 SNe托管在星系中，有SBF距离测量。应用分层贝叶斯方法，我们校准了超新星Ia的峰值亮度，并通过使用96个超新星Ia的红移范围为0.02 < z < 0.075，这是从合并的万神殿样品中提取的样本扩展到哈勃流的哈勃图。我们估计H 0的值= 70.50 ± 2.37（统计）± 3.38（系统）km s−1 Mpc−1（即，百分之三点四，4.8%系统），这与使用红巨星分支的尖端校准获得的值一致。在误差范围内，它也与用造父变星校准的超新星Ia获得的值或从宇宙微波背景分析中推断的值一致。我们发现用SBF标定的SNe Ia距离模量比用造父变星标定的平均大0.07等。我们的研究结果指出，SNe在不同类型的星系之间可能存在差异，这可能源于不同的本地环境和/或祖属性的SNe Ia。采样不同的宿主星系类型，SBF提供了一个补充的方法来使用造父变星，这是重要的，在解决可能的系统学。由于SBF方法有能力达到比造父变星更大的距离，维拉C。鲁宾天文台和JWST的投入运行将增加可以测量SBF距离的星系中的SNe Ia的数量，使SBF测量对于改善SNe Ia的校准以及H 0的估计具有吸引力。
We present a new calibration of the peak absolute magnitude of Type Ia supernovae (SNe Ia) based on the surface brightness fluctuations (SBF) method, aimed at measuring the value of the Hubble constant. We build a sample of calibrating anchors consisting of 24 SNe hosted in galaxies that have SBF distance measurements. Applying a hierarchical Bayesian approach, we calibrate the SN Ia peak luminosity and extend the Hubble diagram into the Hubble flow by using a sample of 96 SNe Ia in the redshift range 0.02 < z < 0.075, which was extracted from the Combined Pantheon Sample. We estimate a value of H0 = 70.50 ± 2.37 (stat.) ± 3.38 (sys.) km s−1 Mpc−1 (i.e., 3.4% stat., 4.8% sys.), which is in agreement with the value obtained using the tip of the red giant branch calibration. It is also consistent, within errors, with the value obtained from SNe Ia calibrated with Cepheids or the value inferred from the analysis of the cosmic microwave background. We find that the SNe Ia distance moduli calibrated with SBF are on average larger by 0.07 mag than those calibrated with Cepheids. Our results point to possible differences among SNe in different types of galaxies, which could originate from different local environments and/or progenitor properties of SNe Ia. Sampling different host galaxy types, SBF offers a complementary approach to using Cepheids, which is important in addressing possible systematics. As the SBF method has the ability to reach larger distances than Cepheids, the impending entry of the Vera C. Rubin Observatory and JWST into operation will increase the number of SNe Ia hosted in galaxies where SBF distances can be measured, making SBF measurements attractive for improving the calibration of SNe Ia, as well as in the estimation of H0.