Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing

White, Martin; Zhou, Rongpu; DeRose, Joseph; Ferraro, Simone; Chen, Shi-Fan; Kokron, Nickolas; Bailey, Stephen; Brooks, David; García-Bellido, Juan; Guy, Julien; Honscheid, Klaus; Kehoe, Robert; Kremin, Anthony; Levi, Michael; Palanque-Delabrouille, Nathalie; Poppett, Claire; Schlegel, David; Tarle, Gregory

doi:10.1088/1475-7516/2022/02/007

Title: Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing

Journal Article · 02 February 2022 · Journal of Cosmology and Astroparticle Physics

DOI: https://doi.org/10.1088/1475-7516/2022/02/007 · OSTI ID:1876398

White, Martin ^[1]; Zhou, Rongpu ^[2]; DeRose, Joseph ^[2]; Ferraro, Simone ^[2]; Chen, Shi-Fan ^[1]; Kokron, Nickolas ^[3]; Bailey, Stephen ^[2]; Brooks, David ^[4]; García-Bellido, Juan ^[5]; Guy, Julien ^[2]; Honscheid, Klaus ^[6]; Kehoe, Robert ^[7]; Kremin, Anthony ^[2]; Levi, Michael ^[2]; Palanque-Delabrouille, Nathalie ^[2]; Poppett, Claire ^[2]; Schlegel, David ^[2]; Tarle, Gregory ^[8]

Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Stanford Univ., CA (United States)
Univ. College London (United Kingdom)
Univ. Autónoma de Madrid (Spain)
The Ohio State Univ., Columbus, OH (United States)
Southern Methodist Univ., Dallas, TX (United States)
Univ. of Michigan, Ann Arbor, MI (United States)

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 ΛCDM, combining all 4 samples and using priors on the background cosmology from supernova and baryon acoustic oscillation measurements, we find S₈ = σ₈(Ωm/0.3)^0.5 = 0.73 ± 0.03. This result is lower than the prediction of the ΛCDM model conditioned on the Planck data. Furthermore, our data prefer a slower growth of structure at low redshift than the model predictions, though at only modest significance.

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Research Organization:: Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Univ. of Michigan, Ann Arbor, MI (United States)

Sponsoring Organization:: USDOE Office of Science (SC), High Energy Physics (HEP)

Grant/Contract Number:: AC02-05CH11231; SC0019193

OSTI ID:: 1876398

Journal Information:: Journal of Cosmology and Astroparticle Physics, Journal Name: Journal of Cosmology and Astroparticle Physics Journal Issue: 02 Vol. 2022; ISSN 1475-7516

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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