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Title: Hyper Suprime-Cam Year 3 results: Cosmology from cosmic shear power spectra

Journal Article · · Physical Review. D.
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  1. Princeton Univ., NJ (United States)
  2. Carnegie Mellon Univ., Pittsburgh, PA (United States); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  3. Univ. of Bonn (Germany); Princeton Univ., NJ (United States)
  4. Univ. of Edinburgh, Scotland (United Kingdom). The Royal Observatory
  5. Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  6. Carnegie Mellon Univ., Pittsburgh, PA (United States)
  7. Carnegie Mellon Univ., Pittsburgh, PA (United States); Argonne National Laboratory (ANL), Argonne, IL (United States)
  8. Inter-University Centre for Astronomy and Astrophysics (IUCAA), Pune (India); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  9. Nagoya Inst. of Technology (Japan); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  10. National Inst. of Natural Sciences (NINS), Tokyo (Japan). National Astronomical Observatory of Japan; Inst. of Statistical Mathematics, Tokyo (Japan)
  11. Hirosaki Univ. (Japan)
  12. Chiba Univ. (Japan)
  13. National Inst. of Natural Sciences (NINS), Tokyo (Japan). National Astronomical Observatory of Japan
  14. Chiba Univ. (Japan); Nagoya Inst. of Technology (Japan); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  15. Gifu Shotoku Gakuen Univ. (Japan); Nagoya Univ. (Japan)
  16. Stanford Univ., CA (United States). Kavli Institute for Particle Astrophysics & Cosmology; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Princeton Univ., NJ (United States)
  17. Univ. of Arizona, Tucson, AZ (United States); Nagoya Univ. (Japan)
  18. Univ. of Oxford (United Kingdom)
  19. Brookhaven National Laboratory (BNL), Upton, NY (United States)
  20. Univ. of Science and Technology of China, Hefei (China). CAS Key Lab. for Researches in Galaxies and Cosmology
  21. Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)
  22. Academia Sinica, Taipei (Taiwan)
  23. Hosei Univ., Tokyo (Japan)
  24. National Astronomical Observatory of Japan, Hilo, HI (United States). Subaru Telescope
  25. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
  26. Kyoto Univ. (Japan); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI); Kyoto Sangyo Univ. (Japan)

Here, we measure weak lensing cosmic shear power spectra from the 3-year galaxy shear catalog of the Hyper Suprime-Cam (HSC) Subaru Strategic Program imaging survey. The shear catalog covers 416 deg2 of the northern sky, with a mean i-band seeing of 0.59 arcsec and an effective galaxy number density of 15 arcmin—2 within our adopted redshift range. With an i-band magnitude limit of 24.5 mag, and four tomographic redshift bins spanning 0.3 ≤ zph ≤ 1.5 based on photometric redshifts, we obtain a high-significance measurement of the cosmic shear power spectra, with a signal-to-noise ratio of approximately 26.4 in the multipole range 300 < ℓ < 1800. The accuracy of our power spectrum measurement is tested against realistic mock shear catalogs, and we use these catalogs to get a reliable measurement of the covariance of the power spectrum measurements. We use a robust blinding procedure to avoid confirmation bias, and model various uncertainties and sources of bias in our analysis, including point spread function systematics, redshift distribution uncertainties, the intrinsic alignment of galaxies and the modeling of the matter power spectrum. For a flat Λ CDM model, we find S8 ≡ σ8m/0.3)0.5 = $${0.776}_{—0.033}^{+0.032}$$, which is in excellent agreement with the constraints from the other HSC Year 3 cosmology analyses, as well as those from a number of other cosmic shear experiments. This result implies a ~2σ-level tension with the Planck 2018 cosmology. We study the effect that various systematic errors and modeling choices could have on this value, and find that they can shift the best-fit value of S8 by no more than ~ 0.5σ, indicating that our result is robust to such systematics.

Research Organization:
Brookhaven National Laboratory (BNL), Upton, NY (United States); Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
Sponsoring Organization:
USDOE Office of Science (SC), High Energy Physics (HEP); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA)
Contributing Organization:
Hyper Suprime-Cam (HSC) Collaboration
Grant/Contract Number:
SC0012704; SC0010118; AC02-76SF00515
OSTI ID:
2315633
Report Number(s):
BNL--225337-2024-JAAM
Journal Information:
Physical Review. D., Journal Name: Physical Review. D. Journal Issue: 12 Vol. 108; ISSN 2470-0010
Publisher:
American Physical Society (APS)Copyright Statement
Country of Publication:
United States
Language:
English

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