Toward neutrino mass from cosmology without optical depth information

Yu, Byeonghee; Knight, Robert Z; Sherwin, Blake D.; Ferraro, Simone; Knox, L.; Schmittfull, Marcel

doi:10.1103/physrevd.107.123522

Cited by 4 publications

(2 citation statements)

References 29 publications

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“…Moving forward, the rapid increase in CMB lensing map noise will allow for a considerable improvement in constraints compared to current analyses using Planck CMB lensing. Assuming 13,000 sq deg of overlap between the CMB maps from Chile-based CMB experiments and the LRG, we expect the cross-correlation constraints of [1] to improve by a factor ≈ 1.4, 2 and 2.5 with ACT, Simons Observatory and CMB-S4 [39] respectively, 5 leading to percent-level constraints on the amplitude of fluctuations at low redshift and shedding light on dark energy [40] and neutrino masses [41], testing our understanding of gravity and weighing in on the "low S 8 " discrepancy [42].…”

Section: Jcap11(2023)097mentioning

confidence: 97%

DESI luminous red galaxy samples for cross-correlations

Zhou,

Ferraro,

White

et al. 2023

J. Cosmol. Astropart. Phys.

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We present two galaxy samples, selected from DESI Legacy Imaging Surveys (LS) DR9, with approximately 20,000 square degrees of coverage and spectroscopic redshift distributions designed for cross-correlations such as with CMB lensing, galaxy lensing, and the Sunyaev-Zel'dovich effect. The first sample is identical to the DESI Luminous Red Galaxy (LRG) sample, and the second sample is an extended LRG sample with 2–3 times the DESI LRG density. We present the improved photometric redshifts, tomographic binning and their spectroscopic redshift distributions and imaging systematics weights, and magnification bias coefficients. The catalogs and related data products will be made publicly available. The cosmological constraints using this sample and Planck lensing maps are presented in a companion paper. We also make public the new set of general-purpose photometric redshifts trained using DESI spectroscopic redshifts, which are used in this work, for all galaxies in LS DR9.

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Section: Jcap11(2023)097mentioning

confidence: 97%

DESI luminous red galaxy samples for cross-correlations

Zhou,

Ferraro,

White

et al. 2023

J. Cosmol. Astropart. Phys.

Self Cite

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“…Indeed, both of these qualities are common to multi-tracer approaches to measuring the neutrino mass with large-scale structure[39][40][41][42][43].…”

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confidence: 99%

Neutrino winds on the sky

Nascimento,

Loverde

2023

J. Cosmol. Astropart. Phys.

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We develop a first-principles formalism to compute the distortion to the relic neutrino density field caused by the peculiar motions of large-scale structures. This distortion slows halos down due to dynamical friction, causes a local anisotropy in the neutrino-CDM cross-correlation, and reduces the global cross-correlation between neutrinos and CDM. The local anisotropy in the neutrino-CDM cross-spectrum is imprinted in the three point cross-correlations of matter and galaxies, or the bispectrum in Fourier space, producing a signal peaking at squeezed triangle configurations. This bispectrum signature of neutrino masses is not limited by cosmic variance or potential inaccuracies in the modeling of complicated nonlinear and galaxy formation physics, and it is not degenerate with the optical depth to reionization. We show that future surveys have the potential to detect the distortion bispectrum.

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No νs is Good News

Craig,

Green,

Meyers

et al. 2024

J. High Energ. Phys.

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The baryon acoustic oscillation (BAO) analysis from the first year of data from the Dark Energy Spectroscopic Instrument (DESI), when combined with data from the cosmic microwave background (CMB), has placed an upper-limit on the sum of neutrino masses, ∑mν< 70 meV (95%). In addition to excluding the minimum sum associated with the inverted hierarchy, the posterior is peaked at ∑mν = 0 and is close to excluding even the minumum sum, 58 meV at 2σ. In this paper, we explore the implications of this data for cosmology and particle physics. The sum of neutrino mass is determined in cosmology from the suppression of clustering in the late universe. Allowing the clustering to be enhanced, we extended the DESI analysis to ∑mν< 0 and find ∑mν =160±90 meV (68%), and that the suppression of power from the minimum sum of neutrino masses is excluded at 99% confidence. We show this preference for negative masses makes it challenging to explain the result by a shift of cosmic parameters, such as the optical depth or matter density. We then show how a result of ∑mν = 0 could arise from new physics in the neutrino sector, including decay, cooling, and/or time-dependent masses. These models are consistent with current observations but imply new physics that is accessible in a wide range of experiments. In addition, we discuss how an apparent signal with ∑mν< 0 can arise from new long range forces in the dark sector or from a primordial trispectrum that resembles the signal of CMB lensing.

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Toward neutrino mass from cosmology without optical depth information

Cited by 4 publications

References 29 publications

DESI luminous red galaxy samples for cross-correlations

DESI luminous red galaxy samples for cross-correlations

Neutrino winds on the sky

No νs is Good News

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