期刊
JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
卷 -, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/1475-7516/2022/02/007
关键词
cosmological parameters from CMBR; cosmological parameters from LSS; gravitational lensing; redshift surveys
资金
- DOE [DE-AC02-05CH11231]
- NSF
- Lawrence Berkeley National Laboratory Chamberlain Fellowship
- Physics Division of Lawrence Berkeley National Laboratory
- Office of Science, Office of High Energy Physics of the U.S. Department of Energy [DE-AC02-05CH11231]
- National Energy Research Scientific Computing Center, a DOE Office of Science User Facility [DE-AC02-05CH11231]
- U.S. National Science Foundation, Division of Astronomical Sciences [AST-0950945]
- Science and Technologies Facilities Council of the United Kingdom
- Gordon and Betty Moore Foundation
- Heising-Simons Foundation
- French Alternative Energies and Atomic Energy Commission (CEA)
- National Council of Science and Technology of Mexico
- Ministry of Economy of Spain
- DOE
Using luminous red galaxies selected from imaging surveys for targeting by the Dark Energy Spectroscopic Instrument (DESI) in combination with CMB lensing maps from the Planck collaboration, researchers probed the amplitude of large-scale structure over 0.4 <= z <= 1. Their findings suggest a slower growth of structure at low redshift than model predictions, with only modest significance.
We use luminous red galaxies selected from the imaging surveys that are being used for targeting by the Dark Energy Spectroscopic Instrument (DESI) in combination with CMB lensing maps from the Planck collaboration to probe the amplitude of large-scale structure over 0.4 <= z <= 1. Our galaxy sample, with an angular number density of approximately 500 deg(-2) over 18,000 sq.deg., is divided into 4 tomographic bins by photometric redshift and the redshift distributions are calibrated using spectroscopy from DESI. We fit the galaxy autospectra and galaxy-convergence cross-spectra using models based on cosmological perturbation theory, restricting to large scales that are expected to be well described by such models. Within the context of ACDM, combining all 4 samples and using priors on the background cosmology from supernova and baryon acoustic oscillation measurements, we find S-8 = sigma(8)(Omega(m)/0.3)(0.5) = 0.73 +/- 0.03. This result is lower than the prediction of the ACDM model conditioned on the Planck data. Our data prefer a slower growth of structure at low redshift than the model predictions, though at only modest significance.
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