Solar neutrinos enable self-calibration of the ν_e + 40Ar cross section to ≲2% in 9-15 MeV via known 8B flux, survival probability, and distinctive Fermi/Gamow-Teller angular distributions.
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NuFit-6.0: Updated global analysis of three-flavor neutrino oscillations
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We present an updated global analysis of neutrino oscillation data as of September 2024. The parameters $\theta_{12}$, $\theta_{13}$, $\Delta m^2_{21}$, and $|\Delta m^2_{3\ell}|$ ($\ell = 1,2$) are well-determined with relative precision at $3\sigma$ of about 13\%, 8\%, 15\%, and 6\%, respectively. The third mixing angle $\theta_{23}$ still suffers from the octant ambiguity, with no clear indication of whether it is larger or smaller than $45^\circ$. The determination of the leptonic CP phase $\delta_{CP}$ depends on the neutrino mass ordering: for normal ordering the global fit is consistent with CP conservation within $1\sigma$, whereas for inverted ordering CP-violating values of $\delta_{CP}$ around $270^\circ$ are favored against CP conservation at more than $3.6\sigma$. While the present data has in principle $2.5$--$3\sigma$ sensitivity to the neutrino mass ordering, there are different tendencies in the global data that reduce the discrimination power: T2K and NOvA appearance data individually favor normal ordering, but they are more consistent with each other for inverted ordering. Conversely, the joint determination of $|\Delta m^2_{3\ell}|$ from global disappearance data prefers normal ordering. Altogether, the global fit including long-baseline, reactor and IceCube atmospheric data results into an almost equally good fit for both orderings. Only when the $\chi^2$ table for atmospheric neutrino data from Super-Kamiokande is added to our $\chi^2$, the global fit prefers normal ordering with $\Delta\chi^2 = 6.1$. We provide also updated ranges and correlations for the effective parameters sensitive to the absolute neutrino mass from $\beta$-decay, neutrinoless double-beta decay, and cosmology.
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- abstract We present an updated global analysis of neutrino oscillation data as of September 2024. The parameters $\theta_{12}$, $\theta_{13}$, $\Delta m^2_{21}$, and $|\Delta m^2_{3\ell}|$ ($\ell = 1,2$) are well-determined with relative precision at $3\sigma$ of about 13\%, 8\%, 15\%, and 6\%, respectively. The third mixing angle $\theta_{23}$ still suffers from the octant ambiguity, with no clear indication of whether it is larger or smaller than $45^\circ$. The determination of the leptonic CP phase $\delta_{CP}$ depends on the neutrino mass ordering: for normal ordering the global fit is consistent
- dataset IO :m 3 = 0, m 1 = q |∆m2 31|, m 2 = q |∆m2 31|+ ∆m 2 21. (9) The observable related to the end point of the beta decay spectrum is [15] m2 β = X i |Uei|2m2 i ,(10) withU ei the PMNS matrix elements in the electron row. Using the recent JUNO results for the solar sector [97], together with the NuFIT 6.0 best-fit values for the re- maining oscillation parameters [98], we find for Eq. (10) and the sum of the neutrino masses: NO :m β = 8.85+0.59 −0.57 meV, X i mi = 58.79+1.07 −1.04 meV, IO :m β = 4
- background 5 500, [arXiv:2511.00157]. [77] M. Escudero and S. J. Witte,A CMB search for the neutrino mass mechanism and its relation to the Hubble tension, Eur. Phys. J. C80(2020), no. 4 294, [arXiv:1909.04044]. [78]Super-KamiokandeCollaboration, K. Bayset. al.,Supernova Relic Neutrino Search at Super-Kamiokande, Phys. Rev. D85(2012) 052007, [arXiv:1111.5031]. 21 [79]Super-KamiokandeCollaboration, H. Zhanget. al.,Supernova Relic Neutrino Search with Neutron Tagging at Super-Kamiokande-IV, Astropart. Phys.6
- background where the quantityεi can be expressed in terms of the Dirac masses of νi,miD, arising from the second term of Eq. (4.1a) - see Ref. [77]. Moreover, employing the ty pe I seesaw formula we can then obtain the light-neutrino mass matrix mν in terms of miD andMiN c . As a consequence, nTL can be nicely linked to low energy neutrino data. We take as inputs the rece ntly updated best-fit values [135] - cf. Ref. [77] - on the neutrino oscillation parameters includin g IceCube IC24 with Super Kamiokande
- dataset White, (2025), arXiv:2511.01779 [astro-ph.CO]. [167] I. Esteban, M. C. Gonzalez-Garcia, M. Maltoni, I. Martinez-Soler, J. P. Pinheiro, and T. Schwetz, JHEP12, 216 (2024), arXiv:2410.05380 [hep-ph]. [168] N. Palanque-Delabrouille, C. Y` eche, N. Sch¨ oneberg, J. Lesgourgues, M. Walther, S. Chaban- ier, and E. Armengaud, JCAP04, 038 (2020), arXiv:1911.09073 [astro-ph.CO]. [169] S. Alamet al.(eBOSS), Phys. Rev. D103, 083533 (2021), arXiv:2007.08991 [astro-ph.CO]. [170] C. D. Froggatt and H. B. Niel
- background somewhere, we will finally discover the new physics able to address the puzzle of the origin of matter in the universe (dark matter and matter-antimatter asymmetry) and the origin of neutrino masses. As stated in the figure, neutrinos might play an important role in addressing some of the cosmological anomalies and tensions. 2. Neutrino mass tension Neutrino oscillation experiments place a lower bound on the sum of neutrino masses [3] ∑︁ 𝑖 𝑚𝜈𝑖 ≥58 meV(95 % C.L.).(1) From cosmological observation
- method This data consists of 13.6×1020 POT in the neutrino mode. The target material is CH 2, and we use 14 logarithmically-spaced energy bins. The NOvA flux peaks around 2 GeV where resonance pro- duction dominates the cross section. To simulate NC events at DUNE, we follow the simu- lation framework from Ref. [41]. We adopt the Technical Design Report (TDR) configuration [13] with a 40 kton LArTPC far detector and a ND LAr fiducial volume of 67 t. The target is argon (18 protons, 22 neutrons per nucl
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A sterile neutrino with a novel density-dependent matter potential Vs resolves multiple oscillation anomalies when Vs is negative and mixing angles are small.
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Complementarity Between Neutrino Neutral and Charged Current Events in the Search for New Physics
Neutral-current events supply sensitivity to isovector NSI parameters that charged-current analyses suppress, enabling the first bounded long-baseline constraints and resolution of individual quark couplings when the two datasets are combined.