4.2 Article

Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements

Journal

JOURNAL OF HIGH ENERGY ASTROPHYSICS
Volume 36, Issue -, Pages 1-26

Publisher

ELSEVIER
DOI: 10.1016/j.jheap.2022.07.002

Keywords

Neutrinos; Cosmic microwave background; Large-scale structure

Funding

  1. Vetenskapsradet (Swedish Research Council) [638-2013-8993]
  2. Oskar Klein Centre for Cosmoparticle Physics
  3. Isaac Newton Trust
  4. Kavli Foundation through a Newton-Kavli Fellowship
  5. Foundation Blanceflor Boncompagni Ludovisi, nee Bildt
  6. Physics Department at Michigan Technological University
  7. Jeff and Gail Kodosky Chair of Physics at the University of Texas, Austin
  8. U.S. Department of Energy Office of Science, Office of High Energy Physics program [DE-SC0022021]
  9. U.S. Department of Energy (DOE) [DE-SC0022021] Funding Source: U.S. Department of Energy (DOE)

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This study revisits cosmological constraints on the sum of the neutrino masses and improves upon previous research by combining BOSS galaxy clustering and Planck CMB data. The results provide an upper limit on the sum of the neutrino masses when combining these measurements with the Planck CMB data. The study also discusses the comparable information content between the full-shape information and the geometrical information of the BAO peaks in the galaxy clustering data, and performs robustness tests on bias and shot noise parameters.
We revisit cosmological constraints on the sum of the neutrino masses Sigma(mv) from a combination of full-shape BOSS galaxy clustering [P(k)] data and measurements of the cross-correlation between Planck Cosmic Microwave Background (CMB) lensing convergence and BOSS galaxy overdensity maps [C-l(kg)], using a simple but theoretically motivated model for the scale-dependent galaxy bias in auto- and cross-correlation measurements. We improve upon earlier related work in several respects, particularly through a more accurate treatment of the correlation and covariance between P(k) and C-l(kg) measurements. When combining these measurements with Planck CMB data, we find a 95% confidence level upper limit of Sigma(mv) < 0.14eV, while slightly weaker limits are obtained when including small-scale ACTPol CMB data, in agreement with our expectations. We confirm earlier findings that (once combined with CMB data) the full-shape information content is comparable to the geometrical information content in the reconstructed BAO peaks given the precision of current galaxy clustering data, discuss the physical significance of our inferred bias and shot noise parameters, and perform a number of robustness tests on our underlying model. While the inclusion of C-l(kg) measurements does not currently appear to lead to substantial improvements in the resulting Sigma(mv) constraints, we expect the converse to be true for near-future galaxy clustering measurements, whose shape information content will eventually supersede the geometrical one. (C) 2022 Elsevier B.V. All rights reserved.

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