Статья

The Pantheon+ Analysis: Cosmological Constraints

Dillon BroutCenter for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]D. ScolnicDepartment of Physics, Duke University, Durham, NC, 27708, USAB PopovicDepartment of Physics, Duke University, Durham, NC, 27708, USAAdam G. RiessDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 USAAnthony CarrSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaJoe ZuntzInstitute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UKRick KesslerDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USAT. M. DavisSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaS. R. HintonSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaD. O. JonesDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USAW. D. KenworthyDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 USAErik R. PetersonDepartment of Physics, Duke University, Durham, NC, 27708, USAKhaled SaidSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaG. TaylorResearch School of Astronomy and Astrophysics, Australian National University, Canberra, AustraliaNoor AliUme University, SE-901 87, Ume, SwedenP. ArmstrongMt. Stromlo Observatory, The Research School of Astronomy and Astrophysics, Australian National University, ACT 2601, AustraliaPranav CharvuDepartment of Physics, Duke University, Durham, NC, 27708, USAArianna DwomohDepartment of Physics, Duke University, Durham, NC, 27708, USACole MeldorfDepartment of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USAA. PalmeseDepartment of Physics, University of California, Berkeley, CA 94720-7300, USAHelen QuDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USABenjamin RoseDepartment of Physics, Duke University, Durham, NC, 27708, USAB. SánchezDepartment of Physics, Duke University, Durham, NC, 27708, USAC. W. StubbsCenter for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]M. VincenziDepartment of Physics, Duke University, Durham, NC, 27708, USACharlotte M. WoodDepartment of Physics and Astronomy, University of Notre Dame, Notre Dame, IN 46556, USAPeter J. BrownDepartment of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX 77843, USAR ChenDepartment of Physics, Duke University, Durham, NC, 27708, USAK. C. ChambersInstitute of Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAD. A. CoulterDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USAMi DaiDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 USAG. DimitriadisSchool of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, IrelandA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAR. J. FoleyDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USASaurabh W. JhaDepartment of Physics and Astronomy, Rutgers, the State University of New Jersey, Piscataway, NJ 08854, USAL KelseyInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UKR. KirshnerCenter for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]A. MöllerCentre for Astrophysics & Supercomputing, Swinburne University of Technology, Victoria 3122, AustraliaJ. MuirPerimeter Institute for Theoretical Physics, 31 Caroline Street North, Waterloo, ON N2L 2Y5, CanadaS. NadathurDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UKY. C. PanGraduate Institute of Astronomy, National Central University, 32001 Jhongli, TaiwanA. RestSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAC. Rojas-BravoDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USAM. ŠakoDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAM. R. SiebertDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USAM. SmithUniversité de Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, F-69622, Villeurbanne, FranceBenjamin E. StahlDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAPhil WisemanSchool of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK

2022en

ABI

Аннотация

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 0 CDM 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 = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.978</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.031</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.024</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> 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 = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.9</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> from Pantheon+ SNe Ia alone, H 0 = 73.3 ± 1.1 km s −1 Mpc −1 when including SH0ES Cepheid distances, and w a = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.65</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.32</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.28</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> 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.

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Идентификаторы

DOI: 10.3847/1538-4357/ac8e04

Цитирования и источники

Цитирований: 24Использованных источников: 0

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