The Pantheon+ Analysis: Cosmological Constraints
The Pantheon+ Analysis: Cosmological Constraints
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DOI：
10.3847/1538-4357/ac8e04
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发表时间：
2022-02
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通讯作者：
D. Brout;D. Scolnic;B. Popovic;A. Riess;A. Carr;J. Zuntz;R. Kessler;T. Davis;S. Hinton;David O. Jones;D. W.;Arcy Kenworthy;E. Peterson;K. Said;G. Taylor;Noor Ali;P. Armstrong;Pranav Charvu;Arianna M. Dwomoh;C. Meldorf;A. Palmese;H. Qu;B. Rose;B. Sanchez;C. Stubbs;Marian Vincenzi;C. Wood;P. Brown;Rebecca Chen;K. Chambers;D. Coulter;M. Dai;G. Dimitriadis;A. Filippenko;R. Foley;S. Jha;L. Kelsey;R. Kirshner;A. Möller;J. Muir;S. Nadathur;Yen-Chen Pan;A. Rest;C. Rojas-Bravo;M. Sako;M. Siebert;Matthew C. Smith;B. Stahl;P. Wiseman
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作者：
D. Brout;D. Scolnic;B. Popovic;A. Riess;A. Carr;J. Zuntz;R. Kessler;T. Davis;S. Hinton;David O. Jones;D. W.;Arcy Kenworthy;E. Peterson;K. Said;G. Taylor;Noor Ali;P. Armstrong;Pranav Charvu;Arianna M. Dwomoh;C. Meldorf;A. Palmese;H. Qu;B. Rose;B. Sanchez;C. Stubbs;Marian Vincenzi;C. Wood;P. Brown;Rebecca Chen;K. Chambers;D. Coulter;M. Dai;G. Dimitriadis;A. Filippenko;R. Foley;S. Jha;L. Kelsey;R. Kirshner;A. Möller;J. Muir;S. Nadathur;Yen-Chen Pan;A. Rest;C. Rojas-Bravo;M. Sako;M. Siebert;Matthew C. Smith;B. Stahl;P. Wiseman
我们从1550颗不同Ia型超新星（SNe Ia）的1701条光曲线的Pantheon+分析中提出了宇宙学参数的约束，红移范围从z = 0.001到2.26。这项工作的特点是增加了SNe的多个交叉校准光度系统的样本量，覆盖了更大的红移跨度，并且与原始的万神殿分析相比，改进了系统不确定性的处理，这些共同导致宇宙学约束能力提高了2倍。对于一个平坦的ΛCDM模型，我们发现Ω M = 0.334±0.018从snia单独。对于一个平坦的w0cdm模型，我们仅从超新星Ia测量到w0 = - 0.90±0.14，当包括造父变星宿主距离和协方差（SH0ES）时，h0 = 73.5±1.1 km s - 1 Mpc - 1，当结合宇宙微波背景（CMB）和重子声学振荡（BAO）的普朗克约束时，w0 = - 0.978 - 0.031+0.024；两个w0值都与一个宇宙学常数一致。我们还提供了迄今为止最精确的关于平坦的w0 wa CDM宇宙中暗能量演化的测量结果，并且仅从Pantheon+ SNe Ia测量到wa =−0.1−2.0+0.9，当包括SH0ES造父变星距离时，h0 = 73.3±1.1 km s−1 Mpc−1，当将Pantheon+ SNe Ia与CMB和BAO数据结合时，wa =−0.65−0.32+0.28。最后，我们发现沿距离阶梯使用Ia型超新星的系统不确定性占测量H 0的总不确定性的不到三分之一，并且不能解释当前局部测量和宇宙模型早期宇宙预测之间的“哈勃张力”。
We present constraints on cosmological parameters from the Pantheon+ analysis of 1701 light curves of 1550 distinct Type Ia supernovae (SNe Ia) ranging in redshift from z = 0.001 to 2.26. This work features an increased sample size from the addition of multiple cross-calibrated photometric systems of SNe covering an increased redshift span, and improved treatments of systematic uncertainties in comparison to the original Pantheon analysis, which together result in a factor of 2 improvement in cosmological constraining power. For a flat ΛCDM model, we find Ω M = 0.334 ± 0.018 from SNe Ia alone. For a flat w 0CDM model, we measure w 0 = −0.90 ± 0.14 from SNe Ia alone, H 0 = 73.5 ± 1.1 km s−1 Mpc−1 when including the Cepheid host distances and covariance (SH0ES), and w 0 = −0.978−0.031+0.024 when combining the SN likelihood with Planck constraints from the cosmic microwave background (CMB) and baryon acoustic oscillations (BAO); both w 0 values are consistent with a cosmological constant. We also present the most precise measurements to date on the evolution of dark energy in a flat w 0 w a CDM universe, and measure w a = −0.1−2.0+0.9 from Pantheon+ SNe Ia alone, H 0 = 73.3 ± 1.1 km s−1 Mpc−1 when including SH0ES Cepheid distances, and w a = −0.65−0.32+0.28 when combining Pantheon+ SNe Ia with CMB and BAO data. Finally, we find that systematic uncertainties in the use of SNe Ia along the distance ladder comprise less than one-third of the total uncertainty in the measurement of H 0 and cannot explain the present “Hubble tension” between local measurements and early universe predictions from the cosmological model.