A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team
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DOI：
10.3847/2041-8213/ac5c5b
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发表时间：
2021-12
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通讯作者：
A. Riess;W. Yuan;L. Macri;D. Scolnic;D. Brout;S. Casertano;David O. Jones;Y. Murakami;G. Anand
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作者：
A. Riess;W. Yuan;L. Macri;D. Scolnic;D. Brout;S. Casertano;David O. Jones;Y. Murakami;G. Anand
我们报告了哈勃太空望远镜 (HST) 对 42 个 Ia 型超新星 (SNe Ia) 宿主星系中造父变星的观测结果，用于校准哈勃常数 (H 0)。其中包括过去四十年在红移 z ≤ 0.01 处发现的所有合适超新星 Ia 的完整样本，从 ≥1000 个 HST 轨道收集和校准，是样本大小限制直接测定 H 0 精度的两倍多。造父变星根据盖亚 EDR3 视差、NGC 4258 中的脉泽（此处为造父变星样本的三倍）进行几何校准，并分离大麦哲伦星云中的食双星。这些锚和 SN Ia 宿主中的所有造父变星均使用相同的仪器 (WFC3) 和滤波器（F555W、F814W、F160W）进行测量，以消除零点误差。我们对造父变星光度测定进行了多次验证，并进行了六次背景测定测试，表明造父变星测量在拥挤的背景下是准确的。这些宿主中的超新星 Ia 校准了修订后的 Pantheon+ 编译中的星等-红移关系，此处考虑了所有超新星数据之间的协方差以及与宿主属性和超新星调查的匹配，以否定系统学。我们将 H 0 局部确定的不确定性降低到 1 km s−1 Mpc−1 ，包括系统学。我们提供了近 70 个分析变量的综合结果，以探索 H 0 对锚点选择、SN 巡天、红移范围、造父变星尘埃处理、金属丰度、周期-光度关系形式、SN 颜色、奇异速度校正、样本分岔和膨胀历史同步测量的敏感性。我们来自造父变星-SN Ia 样本的基线结果是 H 0 = 73.04 ± 1.04 km s−1 Mpc−1，其中包括系统不确定性，并且位于所有分析变体的中值附近。我们证明了 SN Ia 主机和 NGC 4258 之间 TRGB HST 测量的一致性，并将它们同时包含在内以产生 72.53 ± 0.99 km s−1 Mpc−1。包含高红移 SNe Ia 产生 H 0 = 73.30 ± 1.04 km s−1 Mpc−1 和 q 0 = -0.51 ± 0.024。我们发现与 ΛCDM 下普朗克宇宙微波背景观测的 H 0 预测存在 5σ 差异，没有迹象表明该差异是由迄今为止考虑的测量不确定性或分析变化引起的。确定 H 0 的直接路径和宇宙学路径之间长期存在的差异的根源仍然未知。
We report observations from the Hubble Space Telescope (HST) of Cepheid variables in the host galaxies of 42 Type Ia supernovae (SNe Ia) used to calibrate the Hubble constant (H 0). These include the complete sample of all suitable SNe Ia discovered in the last four decades at redshift z ≤ 0.01, collected and calibrated from ≥1000 HST orbits, more than doubling the sample whose size limits the precision of the direct determination of H 0. The Cepheids are calibrated geometrically from Gaia EDR3 parallaxes, masers in NGC 4258 (here tripling that sample of Cepheids), and detached eclipsing binaries in the Large Magellanic Cloud. All Cepheids in these anchors and SN Ia hosts were measured with the same instrument (WFC3) and filters (F555W, F814W, F160W) to negate zero-point errors. We present multiple verifications of Cepheid photometry and six tests of background determinations that show Cepheid measurements are accurate in the presence of crowded backgrounds. The SNe Ia in these hosts calibrate the magnitude–redshift relation from the revised Pantheon+ compilation, accounting here for covariance between all SN data and with host properties and SN surveys matched throughout to negate systematics. We decrease the uncertainty in the local determination of H 0 to 1 km s−1 Mpc−1 including systematics. We present results for a comprehensive set of nearly 70 analysis variants to explore the sensitivity of H 0 to selections of anchors, SN surveys, redshift ranges, the treatment of Cepheid dust, metallicity, form of the period–luminosity relation, SN color, peculiar-velocity corrections, sample bifurcations, and simultaneous measurement of the expansion history. Our baseline result from the Cepheid–SN Ia sample is H 0 = 73.04 ± 1.04 km s−1 Mpc−1, which includes systematic uncertainties and lies near the median of all analysis variants. We demonstrate consistency with measures from HST of the TRGB between SN Ia hosts and NGC 4258, and include them simultaneously to yield 72.53 ± 0.99 km s−1 Mpc−1. The inclusion of high-redshift SNe Ia yields H 0 = 73.30 ± 1.04 km s−1 Mpc−1 and q 0 = −0.51 ± 0.024. We find a 5σ difference with the prediction of H 0 from Planck cosmic microwave background observations under ΛCDM, with no indication that the discrepancy arises from measurement uncertainties or analysis variations considered to date. The source of this now long-standing discrepancy between direct and cosmological routes to determining H 0 remains unknown.