Elsevier B.V. : Synergy between cosmological and laboratory searches in neutrino physics

Gerbino, Martina; Tórtola, Mariam; Lorenz, Christiane S.; Saviano, Ninetta; Mena, Olga; Hagstotz, Steffen; Chen, Mu-Chun; Du, Peizhi; Meyers, Joel; Djurcic, Zelimir; Valle, José W.F.; Suliga, Anna M.; Grohs, Evan; Lattanzi, Massimiliano; Brinckmann, Thejs; Martínez-Miravé, Pablo; Wallisch, Benjamin; Blinov, Nikita; Escudero, Miguel; Abazajian, Kevork N.; Takhistov, Volodymyr; Pettus, Walter C.; Loverde, Marilena; Kelly, Kevin J.

doi:10.1016/j.dark.2023.101333

Article
Report number	arXiv:2203.07377 ; FERMILAB-PUB-22-207-V
Title	Synergy between cosmological and laboratory searches in neutrino physics
Related title	Synergy between cosmological and laboratory searches in neutrino physics: a white paper
Author(s)	Gerbino, Martina (UC, Irvine ; INFN, Ferrara) ; Grohs, Evan (Victoria U. ; North Carolina State U.) ; Lattanzi, Massimiliano (Ferrara U. ; INFN, Ferrara) ; Abazajian, Kevork N. (UC, Irvine) ; Blinov, Nikita (Victoria U.) ; Brinckmann, Thejs (Ferrara U. ; INFN, Ferrara) ; Chen, Mu-Chun (UC, Irvine) ; Djurcic, Zelimir (Argonne) ; Du, Peizhi (YITP, Stony Brook) ; Escudero, Miguel (Munich, Tech. U.) ; Hagstotz, Steffen (Munich U. ; Fermilab) ; Kelly, Kevin J. (CERN ; Fermilab) ; Lorenz, Christiane S. (Zurich, ETH) ; Loverde, Marilena (Washington U., Seattle) ; Martínez-Miravé, Pablo (Valencia U., IFIC ; Valencia U.) ; Mena, Olga (Valencia U., IFIC) ; Meyers, Joel (Southern Methodist U.) ; Pettus, Walter C. (Indiana U.) ; Saviano, Ninetta (INFN, Naples ; SSM, Naples) ; Suliga, Anna M. (LBL, Berkeley ; Wisconsin U., Madison) ; Takhistov, Volodymyr (Tokyo U., IPMU) ; Tórtola, Mariam (Valencia U., IFIC ; Valencia U.) ; Valle, José W.F. (Valencia U., IFIC) ; Wallisch, Benjamin (Princeton, Inst. Advanced Study ; UC, San Diego)
Publication	2023-09-22
Imprint	2022-03-14
Number of pages	56
Note	Originally prepared for submission to the Snowmass Community Planning Exercise, 2021; Current version accepted by Physics of the Dark Universe; 136 pages; 9 Figures
In:	Phys. Dark Univ. 42 (2023) pp.101333
In:	2021 Snowmass Summer Study, Seattle, WA, United States, 11 - 20 July 2021, pp.101333
DOI	10.1016/j.dark.2023.101333 (publication)
Subject category	astro-ph.CO ; Astrophysics and Astronomy ; hep-ph ; Particle Physics - Phenomenology
Abstract	The intersection of the cosmic and neutrino frontiers is a rich field where much discovery space still remains. Neutrinos play a pivotal role in the hot big bang cosmology, influencing the dynamics of the universe over numerous decades in cosmological history. Recent studies have made tremendous progress in understanding some properties of cosmological neutrinos, primarily their energy density. Upcoming cosmological probes will measure the energy density of relativistic particles with higher precision, but could also start probing other properties of the neutrino spectra. When convolved with results from terrestrial experiments, cosmology can become even more acute at probing new physics related to neutrinos or even Beyond the Standard Model (BSM). Any discordance between laboratory and cosmological data sets may reveal new BSM physics and/or suggest alternative models of cosmology. We give examples of the intersection between terrestrial and cosmological probes in the neutrino sector, and briefly discuss the possibilities of what different laboratory experiments may see in conjunction with cosmological observatories.
Copyright/License	publication: © 2023-2024 Elsevier B.V. preprint: (License: CC BY 4.0)

$Effect of free-streaming radiation on the CMB temperature power spectrum (adapted from~\cite{Wallisch:2018rzj}). To illustrate the sensitivity of the Planck~2018 temperature data, we also display their $1\sigma$~error bars~\cite{Planck:2019nip}. \textit{Left}: Variation of the CMB~temperature power spectrum~$\mathcal{D}_\ell^{TT} \equiv \ell (\ell+1)/(2\pi)\,C_\ell^{TT}$ as a function of~$\Neff$ for fixed angular size of the sound horizon~$\theta_s$. The dominant exponential damping of~$\mathcal{D}_\ell^{TT}$ is clearly visible and would be the same if the radiation was non-free-streaming, in contrast to the phase shift illustrated in the right panel. \textit{Right}: Variation of the undamped CMB~temperature power spectrum $\mathcal{K}_\ell = d^{-1}_\ell \mathcal{D}_\ell^{TT}$, with exponential damping function~$d_\ell$, as a function of~$\Neff$. Following~\cite{Follin:2015hya}, the physical baryon density~$\omega_b$, the scale factor at matter-radiation equality $a_\mathrm{eq} \equiv \omega_m/\omega_r$, the angular size of the sound horizon~$\theta_s$ and the angular size of the damping scale~$\theta_D$ are held fixed in the second panel. In addition, the spectra are normalized at the fourth peak. The remaining variation is the phase shift~$\phi$ with a zoom-in shown in the bottom panel. We refer to~\cite{Wallisch:2018rzj} for additional details.$ $Left: Suppression of the matter power spectrum due to massive neutrinos at selected redshifts computed with \texttt{CLASS}~\cite{Blas:2011rf}. The comparison is made at fixed $H_0$, $\Omega_\mathrm{m} h^2$, $\Omega_\mathrm{b} h^2$, and $A_s$. Right: Relative suppression effect on the power spectrum at $z=0$ caused by neutrinos with varying total mass $\sum m_\nu$, with parameters $\Omega_c$, $\Omega_b$ and $H_0$ kept constant. Large-scale structure experiments have little sensitivity at scales $k < 10^{-2} h/\mathrm{Mpc}$ and can mostly resolve the suppressed part of the spectrum.$ $Left: Suppression of the matter power spectrum at $z=0$ for varying neutrino mass relative to a reference cosmology with massless neutrinos. Large-scale structure experiments have little sensitivity at scales $k < 10^{-2} h/\mathrm{Mpc}$ and can mostly resolve the suppressed part of the spectrum. Right: Evolution of the suppression of the matter power spectrum for fixed neutrino mass $\sum m_i = 60 \, \mathrm{meV}$ with redshift. The evolution is mild and the suppression slightly increases with time as neutrinos dampen the growth of structures. All comparisons are made keeping physical densities $\Omega_i h^2$ and $h$ fixed.$ Show more plots

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