The Pantheon+ Analysis: Cosmological Constraints
Filippenko, Alexei V.; Coulter, David A.; Foley, Ryan J.; Pan, Yen-Chen; Rest, Armin; Riess, Adam G.; Kirshner, Robert P.; Chambers, Ken; Jones, David; Scolnic, Dan; Stubbs, Christopher W.; Sako, Masao; Brout, Dillon; Said, Khaled; Stahl, Benjamin E.; Möller, Anais; Zuntz, Joe; Dimitriadis, Georgios; Armstrong, Patrick; Jha, Saurabh W.; Siebert, Matthew R.; Brown, Peter J.; Palmese, Antonella; Dai, Mi; Wood, Charlotte M.; Davis, Tamara M.; Nadathur, Seshadri; Kenworthy, W. D'Arcy; Peterson, Erik R.; Taylor, Georgie; Rose, Benjamin M.; Vincenzi, Maria; Dwomoh, Arianna; Ali, Noor; Qu, Helen; Carr, Anthony; Popovic, Brodie; Kessler, Rick; Hinton, Samuel; Charvu, Pranav; Meldorf, Cole; Sanchez, Bruno; Chen, Rebecca; Kelsey, Lisa; Muir, Jessie; Rojas-Bravo, Cesar; Smith, Mat; Wiseman, Phil
United States, Australia, United Kingdom, Sweden, Ireland, France, Canada, Taiwan
Abstract
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.