Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Joe Zuntz, Rick Kessler, Anthony Carr, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworth… 展开作者
Dillon Brout, Dan Scolnic, Brodie Popovic, Adam G. Riess, Joe Zuntz, Rick Kessler, Anthony Carr, Tamara M. Davis, Samuel Hinton, David Jones, W. D'Arcy Kenworthy, Erik R. Peterson, Khaled Said, Georgie Taylor, Noor Ali, Patrick Armstrong, Pranav Charvu, Arianna Dwomoh, Antonella Palmese, Helen Qu, Benjamin M. Rose, Christopher W. Stubbs, Maria Vincenzi, Charlotte M. Wood, Peter J. Brown, Rebecca Chen, Ken Chambers, David A. Coulter, Mi Dai, Georgios Dimitriadis, Alexei V. Filippenko, Ryan J. Foley, Saurabh W. Jha, Lisa Kelsey, Robert P. Kirshner, Anais Möller, Jessie Muir, Seshadri Nadathur, Yen-Chen Pan, Armin Rest, Cesar Rojas-Bravo, Masao Sako, Matthew R. Siebert, Mat Smith, Benjamin E. Stahl, Phil Wiseman
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, increased redshift span, and improved treatment of systematic uncertainties in comparison to the original Pantheon analysis and results in a factor of two improvement in cosmological constraining power. For a Flat$Λ$CDM model, we find $Ω_M=0.334\pm0.018$ from SNe Ia alone. For a Flat$w_0$CDM model, we measure $w_0=-0.90\pm0.14$ from SNe Ia alone, H$_0=73.5\pm1.1$ km s$^{-1}$ Mpc$^{-1}$ when including the Cepheid host distances and covariance (SH0ES), and $w_0=-0.978^{+0.024}_{-0.031}$ when combining the SN likelihood with 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$w_0w_a$CDM universe, and measure $w_a=-0.1^{+0.9}_{-2.0}$ from Pantheon+ alone, H$_0=73.3\pm1.1$ km s$^{-1}$ Mpc$^{-1}$ when including SH0ES, and $w_a=-0.65^{+0.28}_{-0.32}$ when combining Pantheon+ 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.
QCD CP-violation scenario for a revised cosmological dynamics: analysis of the binned Pantheon Sample of Super Novae Ia
ENEA - C. R. Frascati（意大利国家新能源与可再生能源研究中心）；National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）；Space Science Institute（空间科学研究所）
研究修正宇宙动力学，宇宙由重子物质和复标量场构成，构建有效跑动哈勃常数，与 Ia 型超新星潘特heon 样本数据比较，能依理论推测对数据给出满意解释，比 $\Lambda$CDM 模型更受统计青睐。
The Pantheon+ Analysis: Forward-Modeling the Dust and Intrinsic Colour Distributions of Type Ia Supernovae, and Quantifying their Impact on Cosmological Inferences
The Complete Light-curve Sample of Spectroscopically Confirmed Type Ia Supernovae from Pan-STARRS1 and Cosmological Constraints from The Combined Pantheon Sample
我们目前的光学光变曲线，红移和分类的365光谱证实Ia型超新星（SNe Ia）发现的泛星1（PS1）中深调查。我们详细介绍了改进的PS1 SN测光，天体测量和校准，减少系统的不确定性PS1 SN Ia距离。我们将279个PS1 SN Ia（$0.03 < z < 0.68$）的子集与来自SDSS、SNLS、各种低z和HST样本的SN Ia的有用距离估计相结合，以形成SN Ia的最大组合样本，该样本由总共1048个SN Ia组成，范围从$0.01 < z < 2.3$，我们称之为“万神殿样本”。当将普朗克2015 CMB测量与Pantheon SN样本相结合时，我们发现wCDM模型的$Ω_m=0.307\pm0.012$和$w = -1.026\pm0.041$。当SN和CMB约束与BAO和本地H0测量的约束相结合时，分析产生了迄今为止最精确的暗能量测量：w0waCDM模型的$w0 = -1.007\pm 0.089$和$wa = -0.222 \pm0.407$。在PS1样品的统计数据中增加了$2\times$，改进了校准和光度测定，以及更严格的光变曲线质量削减后，以前在PS1和低z SNe的分析中看到的宇宙学常数的张力已经减弱。我们发现，在我们的暗能量的测量系统的不确定性几乎一样大的统计不确定性，主要是由于建模的低红移样本的限制。这一点必须得到解决，以便在未来利用超新星Ia测量暗…
Using Pantheon and DES supernova, baryon acoustic oscillation, and Hubble parameter data to constrain the Hubble constant, dark energy dynamics, and spatial curvature
Constraining and Comparing the Dynamical Dark Energy and f(R) Modified Gravity Models with Cosmological Distance Measurements
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Department of Physics, College of Sciences, Northeastern University（东北大学理学院物理系）
Model-Independent Reconstruction of Quintessence Potential and Kinetic Energy from DESI DR2 and Pantheon+ Supernovae
School of Physics and Optoelectronic Engineering, Yangtze University（长江大学物理与光电工程学院）；Liaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern University（东北大学理学院辽宁省宇宙学与天体物理重点实验室）
Constraints on Newton's Constant from Cosmological Observations
牛顿常数对超新星的CMB功率谱和光变曲线都有观测影响。我们用Planck数据、BAO数据和SNIa测量来约束CMB时期牛顿常数$G$的变化和PANTHEON样品的红移范围，没有发现$G$随红移变化的证据。通过引入一个自由参数$G$扩展$Λ$ CDM模型，得到了68 $\%$ C. L.处的$G =(6.65635_{-0.18560}^{+0.18766} ) \times 10^{-11} \rm m^3kg^{-1}s^{-2}$和$H_0=67.62^{+1.24}_{-1.25} $ km s $^{-1}$ Mpc $^{-1}$.来自普朗克$+$ BAO $+$未校准的万神殿。结果表明，$G$的值与CODATA 2018一致，但无法通过这种方式求解$H_0$张力。
Tightening Cosmological Constraints Within and Beyond $Λ$CDM Using Gamma-Ray Bursts Calibrated with Type Ia Supernovae
INAF - Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究院）；Department of Astronomy, Beijing Normal University（北京师范大学天文系）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Università di Camerino（卡梅里诺大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Istituto Nazionale di Fisica Nucleare, Sezione di Perugia（意大利国家核物理研究所佩鲁贾分部）；SUNY Polytechnic（纽约州立理工大学）；Al-Farabi Kazakh National University（阿里-法拉比哈萨克国立大学）；ICRANet（国际相对论天体物理中心网络）
Alleviating the Hubble Tension with Smooth Sign-Switching Dark Energy: Full CMB Constraints with DESI and PantheonPlus
IKERBASQUE, Basque Foundation for Science（伊卡巴斯基克巴斯克科学基金会）；Department of Physics, University of the Basque Country UPV/EHU（巴斯克大学物理系）；EHU Quantum Center, University of the Basque Country UPV/EHU（巴斯克大学量子中心）；Department of Physics, Southern University of Science and Technology（南方科技大学物理系）
Falsifying $Λ$CDM: Model-independent tests of the concordance model with eBOSS DR14Q and Pantheon
我们结合模型独立重建的膨胀历史，从最新的万神殿超新星距离模量汇编和测量重子声学振荡，以测试宇宙学的和谐模型，即FLRW度量和平坦度的空间曲率的一些重要方面。然后，我们使用重建的扩展历史，以适应红移空间失真的增长测量，并获得强约束$(Ω_\mathrm{m},γ,σ_8)$在一个模型无关的方式。我们的结果表明，与一个空间平坦的FLRW宇宙与广义相对论支配的扰动的结构形成和宇宙学常数作为暗能量的一致性。然而，我们也可以看到一些紧张的暗示，在不同的观测范围内的和谐模型相关的高红移观测（$z > 1$）的膨胀历史。这支持了Sahni et al.（2014）和Zhao et al.（2017）的早期发现，并强调了精确测量膨胀历史和高红移结构增长的重要性。
