We measure the smallscale clustering of the Data Release 16 extended Baryon Oscillation Spectroscopic Survey Luminous Red Galaxy sample, corrected for fibrecollisions using Pairwise Inverse Probability weights, which give unbiased clustering measurements on all scales. We fit to the monopole and quadrupole moments and to the projected correlation function over the separation range $760\, h^{1}{\rm Mpc}$ with a model based on the aemulus cosmological emulator to measure the growth rate of cosmic structure, parametrized by fσ8. We obtain a measurement of fσ8(z = 0.737) = 0.408 ± 0.038, which is 1.4σ lower than the value expected from 2018 Planck data for a flat ΛCDM model, and is more consistent with recent weaklensing measurements. The level of precision achieved is 1.7 times better than more standard measurements made using only the largescale modes of the same sample. We also fit to the data using the full range of scales $0.1\text{}60\, h^{1}{\rm Mpc}$ modelled by the aemulus cosmological emulator and find a 4.5σ tension in the amplitude of the halo velocity field with the Planck + ΛCDM model, driven by a mismatch on the nonlinear scales. This may not be cosmological in origin, and could be due to a breakdown in the Halo Occupation Distribution model used inmore »
This content will become publicly available on February 1, 2023
Cosmological constraints from the tomographic crosscorrelation of DESI Luminous Red Galaxies and Planck CMB lensing
Abstract 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 largescale 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 galaxyconvergence crossspectra 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 ΛCDM, combining all 4 samples and using priors on the background cosmology from supernova and baryon acoustic oscillation measurements, we find S 8 = σ 8 (Ω m /0.3) 0.5 = 0.73 ± 0.03. This result is lower than the prediction of the ΛCDM 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.
 Award ID(s):
 1713791
 Publication Date:
 NSFPAR ID:
 10322138
 Journal Name:
 Journal of Cosmology and Astroparticle Physics
 Volume:
 2022
 Issue:
 02
 ISSN:
 14757516
 Sponsoring Org:
 National Science Foundation
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