Статья

The Pantheon+ Analysis: The Full Data Set and Light-curve Release

D. ScolnicDepartment of Physics, Duke University, Durham, NC 27708, USADillon BroutCenter for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAAnthony CarrSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaAdam G. RiessDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 USAT. M. DavisSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaArianna DwomohDepartment of Physics, Duke University, Durham, NC 27708, USAD. O. JonesDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USANoor AliUmeå University, SE-901 87, Umeå, SwedenPranav CharvuDepartment of Physics, Duke University, Durham, NC 27708, USAR ChenDepartment of Physics, Duke University, Durham, NC 27708, USAErik R. PetersonDepartment of Physics, Duke University, Durham, NC 27708, USAB PopovicDepartment of Physics, Duke University, Durham, NC 27708, USABenjamin RoseDepartment 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, 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, USAK. DettmanDepartment of Physics and Astronomy, Rutgers, the State University of New Jersey, Piscataway, NJ 08854, 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, USAC. D. KilpatrickCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60208, USAR. KirshnerCenter for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAY. C. PanGraduate Institute of Astronomy, National Central University, 32001 Jhongli, TaiwanA. RestSpace Telescope Science Institute, Baltimore, MD 21218, USAC. Rojas-BravoDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USAM. R. SiebertDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 92064, USABenjamin E. StahlDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USA

2022en

ABI

Аннотация

Abstract Here we present 1701 light curves of 1550 unique, spectroscopically confirmed Type Ia supernovae (SNe Ia) that will be used to infer cosmological parameters as part of the Pantheon+ SN analysis and the Supernovae and H 0 for the Equation of State of dark energy distance-ladder analysis. This effort is one part of a series of works that perform an extensive review of redshifts, peculiar velocities, photometric calibration, and intrinsic-scatter models of SNe Ia. The total number of light curves, which are compiled across 18 different surveys, is a significant increase from the first Pantheon analysis (1048 SNe), particularly at low redshift ( z ). Furthermore, unlike in the Pantheon analysis, we include light curves for SNe with z < 0.01 such that SN systematic covariance can be included in a joint measurement of the Hubble constant ( H 0 ) and the dark energy equation-of-state parameter ( w ). We use the large sample to compare properties of 151 SNe Ia observed by multiple surveys and 12 pairs/triplets of “SN siblings”—SNe found in the same host galaxy. Distance measurements, application of bias corrections, and inference of cosmological parameters are discussed in the companion paper by Brout et al., and the determination of H 0 is discussed by Riess et al. These analyses will measure w with ∼3% precision and H 0 with ∼1 km s −1 Mpc −1 precision.

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Идентификаторы

DOI: 10.3847/1538-4357/ac8b7a

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Цитирований: 28Использованных источников: 0

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